Proper Motions of Stars in the Zone Catalogue -40 to -52 degrees of 20843 Stars for 1900 1005 I/5 Proper Motions in Cape Zone Catalogue -40/-52 Proper Motions of Stars in the Zone Catalogue -40 to -52 degrees of 20843 Stars for 1900 J H Spencer J Jackson His Majesty's Stationery Office, London ??? ??? 1936 Positional data Proper motions This catalog, listing the proper motions of 20,843 stars from the Cape Astrographic Zones, was compiled from three series of photographic plates. The plates were taken at the Royal Observatory, Cape of Good Hope, in the following years: 1892-1896, 1897-1910, 1923-1928. Data given include centennial proper motion, photographic and visual magnitude, Harvard spectral type, Cape Photographic Durchmusterung (CPD) identification, epoch, right ascension and declination for 1900.
The catalogue --- Number 5 --- CZC Catalogue Identification Number --- Vmag Visual Magnitude mag RAh Right Ascension for 1900 hours h RAm Right Ascension for 1900 minutes min RAcs Right Ascension seconds in 0.01sec 1900 0.01s DE- Declination Sign --- DEd Declination for 1900 degrees deg DEm Declination for 1900 arcminutes arcmin DEds Declination for 1900 arcseconds 0.1arcsec Ep-1900 Epoch -1900 cyr CPDZone Cape Photographic Durchmusterung Zone --- CPDNo Cape Photographic Durchmusterung Number --- Pmag Photographic Magnitude mag Sp HD Spectral Type --- pmRAs Proper Motion in RA the relation is pmRA = 15 * pmRAs * cos(DE) if pmRAs is expressed in s/yr and pmRA in arcsec/yr 0.1ms/yr pmRA Proper Motion in RA mas/yr pmDE Proper Motion in Dec mas/yr Julie Anne Watko SSDOO/ADC 1995 Nov 03 I_5.xml Catalogue of 20554 Faint Stars in the Cape Astrographic Zone -40 to -52 Degrees for the Equinox of 1900.0 1006 I/6 Cape 20554 Faint Stars, -40 to -52, 1900.0 Catalogue of 20554 Faint Stars in the Cape Astrographic Zone -40 to -52 Degrees for the Equinox of 1900.0 J H Spencer J Jackson His Majesty's Stationery Office, London ??? ??? 1939 1939HMSO..C......0S Positional data Proper motions This catalog contains positions, precessions, proper motions, and photographic magnitudes for 20,554 stars. These were derived from photographs taken at the Royal Observatory, Cape of Good Hope between 1923 and 1928. It covers the astrographic zones -40 degrees to -52 degrees of declination. The positions are given for epoch 1900 (1900.0). It includes spectral types for many of the stars listed. It extends the earlier catalogs derived from the same plates to fainter magnitudes. The computer-readable version consists of a single data table. The stated probable error for the star positions is 0.024 seconds of time (R.A.) and 0.25 seconds of arc (dec.) for stars with one determination, 0.017 seconds of time, and 0.18 seconds of arc for two determinations, and 0.014 / 0.15 for stars with three determinations. The precession and secular variations were derived from Newcomb's constants. The authors quote probable errors of the proper motions in both coordinates of 0.008 seconds of arc for stars with one determination, 0.0055 seconds for stars with two determinations, and 0.0044 for stars with three. The photographic magnitudes were derived from the measured diameters on the photographic plates and from the magnitudes given in the Cape Photographic Durchmusterung. The spectral classification of the cataloged stars was done with the assistance of Annie Jump Cannon of the Harvard College Observatory. The user should consult the source reference for more details of the measurements and reductions. See also the notes in this document for additional information on the interpretation of the entries.
Data ID Cape Number --- rem Remark A = Astrographic Star F = Faint Proper Motion Star N = Other Note --- CPDZone Cape Phot. Durchmusterung (CPD) Zone All CPD Zones are negative. - signs are not included in data. "0" in column 8 signifies Astrographic Plate instead of CPD. --- CPD CPD Number or Astrographic Plate See also note on CPDZone. Astrographic plate listed "is the more southerly on which the star occurs." Thus, y-coordinate is positive wherever possible. --- n_CPD [1234] Remarks A number from 1-4 appears in this byte for double stars where the same CPD number applies to more than one star. --- mpg Photographic Magnitude The Photographic Magnitude is "determined from the CPD Magnitude and the diameter on the Cape Astrographic Plates by means of the data given in the volume on the Magnitudes of Stars in the Cape Zone Catalogue." A null value (99.9) signifies a variable star. mag RAh Mean Right Ascension hours 1900 h RAm Mean Right Ascension minutes 1900 min RAs Mean Right Ascension seconds 1900 s DEd Mean Declination degrees 1900 deg DEm Mean Declination arcminutes 1900 arcmin DEs Mean Declination arcseconds 1900 arcsec N Number of Observations --- Epoch Epoch +1900 yr pmRA Proper Motion in RA seconds of time s/a pmRAas Proper Motion in RA arcseconds arcsec/a pmDE Proper Motion in Dec arcseconds arcsec/a Sp HD Spectral Type --- Julie Anne Watko SSDOO/ADC 1996 Mar 26 I_6.xml Proper Motions of 1160 Late-Type Stars 1014 I/14 Proper Motions of 1160 Late-Type Stars Proper Motions of 1160 Late-Type Stars H J Fogh Olsen Astron. Astrophys. Suppl. Ser. 2 69 1970 1970A&AS....2...69O II/38 : Stars observed photoelectrically by Dickow et al. Fogh Olsen H.J. 1970, Astron. Astrophys. Suppl. Ser., 2, 69. Fogh Olsen H.J. 1970, Astron. Astrophys., Suppl. Ser., 1, 189. Proper motions Improved proper motions for the 1160 stars contained in the photometric catalog by Dickow et al. (1970) are presented. Most of the proper motions are from the GC, transferred to the system of FK4. For stars not included in the GC, preliminary AGK or SAO proper motions are given. Fogh Olsen (Astron. Astrophys. Suppl. Ser., 1, 189, 1970) describes the method of improvement. The mean errors of the centennial proper motions increase with increasing magnitude. In Right Ascension, these range from 0.0043/cos(dec) for very bright stars to 0.096/cos(dec) for the faintest stars. In Dec- lination, the range is from 0.065 to 1.14.
Proper motion data No Number Henry Draper or Bonner Durchmusterung number --- pmRA Centennial Proper Motion RA s/ca pmDE Centennial Proper Motion Dec arcsec/ca RV Radial Velocity km/s Julie Anne Watko ADC 1996 Jun 03 I_14.xml Katalog von 3356 Schwachen Sternen fuer das Aequinoktium 1950 +89 degrees 1016 I/16 Catalog of 3356 Faint Stars, 1950 Katalog von 3356 Schwachen Sternen fuer das Aequinoktium 1950 +89 degrees J Larink A Bohrmann H Kox J Groeneveld H Klauder Verlag der Sternwarte, Hamburg-Bergedorf ??? ??? 1955 1955 Fundamental catalog Positional data Proper motions This catalog of 3356 faint stars was derived from meridian circle observations at the Bergedorf and Heidelberg Observatories. The positions are given for the equinox 1950 on the FK3 system. The stars are mainly between 8.0 and 10.0 visual magnitude. A few are brighter than 8.0 mag. The lower limit in brightness resulted from the visibility of the stars.
All stars were observed at both the Heidelberg and Bergedorf Observatories. Normally, at each observatory, two observations were obtained with the clamp east and two with the clamp west. The mean errors are comparable for the two observatories with no significant systematic difference in the positions between them. The mean errors of the resulting positions should be approximated 0.011s/cos(dec) in right ascension and ).023" in declination. The proper motions were derived from a comparison with the catalog positions with the positions in the AGK2 and AGK2A with a 19 year baseline and from a comparison of new positions with those in Kuestner 1900 with about a fifty year baseline. The magnitudes were taken from the AGK2. Most spectral types were determined by A. N. Vyssotsky. A few are from the Bergedorfer Spektraldurchmusterung.
The catalog ID Catalog number --- DMz BD zone --- DMn BD number --- mag Photographic magnitude mag Sp Spectral class --- RAh Right Ascension hours (1950) h RAm Right Ascension minutes (1950) min RAs Right Ascension seconds (1950) s Pr-RA1 First order precession in RA per century 0.01s/a Pr-RA2 Second order precession in RA per century 0.0001s2/a2 pmRA Proper motion in RA from AGK2 positions 0.01s/a pmRA2 Proper motion in RA from Kuestner positions 0.01s/a DE- Sign of declination (1950) --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin DEs Declination seconds (1950) arcsec Pr-de1 First order precession in dec per century arcsec/ha Pr-de2 Second order precession in dec per century arcsec2/ha2 pmdec Proper motion in DE from AGK2 positions arcsec/ha pmdec2 Proper motion in DE from Kuestner positions arcsec/ha epoch Epoch of observation - 1900.0 yr rem Note for star in printed catalog 1 = ma (blend?) 3 = pr (preceding) 4 = seq (following) 5 = bor (northern) 6 = au (southern) * = other note in printed volume (All notes in the printed volume have not been indicated in this version.) the printed volume sometimes has additional information on the systems with numerical remarks. --- Nancy Grace Roman ADC/SSDOO 1996 Feb 01 I_16.xml Astrographic Catalogue 1021A I/21A AC Toulouse, Bordeaux, Paris & Oxford Astrographic Catalogue P Lacroute A Valbousquet CDS Bull. No. 6, p. 38 ??? ??? 1974 1974BICDS...6...38L Astrographic zones Magnitudes, photographic Positional data The "Carte de Ciel" (or "Astrographic Catalogue") is a catalogue of star positions and magnitudes, determined on the photographic plates taken by the normal astrographs which are installed in observatories of various latitudes, as a world-wide astronomical project (see Eichhorn, 1974, p279). The catalogue is divided into 22 declination zones, each of which is assigned to each observatory, e.g., a zone from +18 to +24 degrees is to Paris observatory. Each observatory has taken photographs of 2 deg x 2 deg area in and covering each zone, measured the X,Y coordinates of star images on the photographic plates, and published the results as the printed catalogues. The present catalogue is the results of reduction of these X,Y coordinates into right ascension and declination values, for declination zones of +05 to +31, by using AGK2/3 catalogue as the reference.
Toulouse zone (+05 to +10 and +11 degree) ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. --- HYPH hyphen number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- STAR running number of star on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- RAh right ascension (hours) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. h RAm right ascension (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. min RAs ascension (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. s DE- declination sign number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- DEd declination (degrees) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. deg DEm declination (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcmin DEs declination (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcsec EPOCH plate epoch number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. a mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. mag AGKNO AGK2 number AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- SUFFIX suffix to the AGK2 number Suffix to the AGK2 number, if needed, otherwise CR/LF. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- Bordeaux zone (+11 to +17 degree) ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. --- HYPH hyphen number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- STAR running number of star on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- RAh right ascension (hours) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. h RAm right ascension (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. min RAs ascension (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. s DE- declination sign number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- DEd declination (degrees) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. deg DEm declination (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcmin DEs declination (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcsec EPOCH plate epoch number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. a mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. mag AGKNO AGK2 number AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- SUFFIX suffix to the AGK2 number Suffix to the AGK2 number, if needed, otherwise CR/LF. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- Paris zone (+18 to +24 degree) ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. --- HYPH hyphen number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- STAR running number of star on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- RAh right ascension (hours) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. h RAm right ascension (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. min RAs ascension (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. s DE- declination sign number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- DEd declination (degrees) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. deg DEm declination (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcmin DEs declination (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcsec EPOCH plate epoch number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. a mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. mag AGKNO AGK2 number AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- SUFFIX suffix to the AGK2 number Suffix to the AGK2 number, if needed, otherwise CR/LF. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- Oxford I zone (+25 to +31 degree) ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. --- HYPH hyphen number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- STAR running number of star on plate Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- RAh right ascension (hours) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. h RAm right ascension (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. min RAs right ascension (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. s DE- declination sign number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- DEd declination (degrees) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. deg DEm declination (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. arcmin DEs declination (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. arcsec EPOCH plate epoch number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. a mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. mag AGKNO AGK2 number, if AGK2/3 star was AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- SUFFIX suffix to the AGK2 number suffix to the AGK2 number, if needed, otherwise CR/LF. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- J.A. Watko SSDOO/ADC 1995 Koichi Nakajima [CDS] 24-Sep-1993 Nov 16 I_21A.xml Astrographic Catalogue 1022A I/22A Astrographic Catalogue Algier, -02 to +04 Astrographic Catalogue P Lacroute A Valbousquet CDS Bull. No. 6, p. 38 ??? ??? 1974 1974BICDS...6...38L Positional data Astrographic zones Magnitudes, photographic The "Carte de Ciel" (or "Astrographic Catalogue") is a catalogue of star positions and magnitudes, determined on the photographic plates taken by the normal astrographs which are installed in observatories of various latitudes, as a world-wide astronomical project (see Eichhorn, 1974, p279). The catalogue is divided into 22 declination zones, each of which is assigned to each observatory, e.g., a zone from +18 to +24 degrees is to Paris observatory. Each observatory has taken photographs of 2 deg x 2 deg area in and covering each zone, measured the X,Y coordinates of star images on the photographic plates, and published the results as the printed catalogues. The present catalogue is the results of reduction of these X,Y coordinates into right ascension and declination values, for declination zones of +05 to +31, by using AGK2/3 catalogue as the reference.
catalog ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that this number is negative when the zone is negative. --- STAR running number of star on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. --- RAmas right ascension (B1950) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. mas DEmas declination (B1950) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. mas EPOCH plate epoch from 180000 number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. ca mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. dmag X X coordinate on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. 0.1um Y Y coordinate on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. 0.1um AGK3Z AGK3 number : zone number No signs on any AGK3 zones. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. deg AGK3N AGK3 number : star number number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. --- ZERO zero number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. --- Koichi Nakajima CDS 1993 J.A. Watko [SSDOO/ADC] 21-Feb-1996 Sep 24 I_22A.xml Results of observations with the nine-inch transit circle 1913-1926. Catalogue of 9989 standard and intermediary stars, Miscellaneous stars. 1040 I/40 WASHINGTON 20 Catalog Results of observations with the nine-inch transit circle 1913-1926. Catalogue of 9989 standard and intermediary stars, Miscellaneous stars. H R Morgan Publ. USNO, 2nd series, vol. XIII, Washington ??? ??? 1933 1983 Meridian observations Positional data Historical catalog This catalogue contains the two parts: the 9989 first stars are the standard and intermediary stars, +90 to -36 degrees of declination, observed in the years 1913 to 1926, and reduced without proper motion to the equinox 1920.0 ; the second part (stars numbered 9990 to 10571) are 582 miscellaneous stars.
The catalog of (9989 + 582) stars. Seq Running number --- DM Durchmusterung (BD or CD) identification --- Sp Spectral type, from HD --- NumSp Coded spectral type number=1 the numeric spectral type exists only for stars 1-10400; it is coded on 3 bytes as follows: ------------------------------- Byte#16 Byte#17 Byte#18 ------------------------------- R=0 a or 0=0 Oe5=1 b or 1=1 O=2 c or 2=2 B=2 d or 3=3 *=3 A=4 e or 4=4 F=5 5=5 e=5 G=6 6=6 K=7 7=7 M=8 8=8 N=9 9=9 S=- p=- ------------------------------- Special cases: Mb=83 Mc=88, Md=8 5, Me=8-5, Np=9 --- Vmag Magnitudes (from Harvard Revised Photometry or corrected BD) mag n_Vmag for variable star --- ObsMag Observed magnitude mag RAh Right Ascension B1920 (hours), at Epoch h RAm Right Ascension B1920 (minutes), at Epoch min RAs Right Ascension B1920 (seconds), at Epoch s pmRA Annual proper motion in RA (in Boss system) s/a DE- Declination B1920 (sign) --- DEd Declination B1920 (degrees) deg DEm Declination B1920 (minutes) arcmin DEs Declination B1920 (0.01arcsec) arcsec pmDE Annual proper motion in Dec (in Boss system) arcsec/a o_RAs Number of observations in RA --- o_DEs Number of observations in Dec number=2 the value is not specified when it is identical to the corresponding number for RA. --- EpRA-1900 Mean Epoch of Right Ascension 0.01a EpDE-1900 Mean Epoch of Declination number=2 the value is not specified when it is identical to the corresponding number for RA. 0.01a Note indicates a note in the catalog --- Francois Ochsenbein, James Marcout CDS 1998 Jun 10 UNKNOWN UNKNOWN The catalogue was originally keypunched at the Astronomisches Rechen-Institut, Heidelberg, Germany, in the 70's. It contained 10400 stars, i.e. 171 stars were missing (note from Richard Swifte, Royal Greenwich Observatory, October 1981). The missing stars were added in June 1998, with the help of an Optical Character Recognition system. I_40.xml Catalogue of Coordinates of Reference Faint, Bright and Double Stars South of -47 Degree and Corrections to FK4 Positions as Observed by Pulkovo Astronomers with the Meridian Circle at the Cerro-Kalan Observatory (Chile) in 1963-1968 1044 I/44 Second Cat of Fundamental Stars Catalogue of Coordinates of Reference Faint, Bright and Double Stars South of -47 Degree and Corrections to FK4 Positions as Observed by Pulkovo Astronomers with the Meridian Circle at the Cerro-Kalan Observatory (Chile) in 1963-1968 G D Baturina V S Bedin K G Gnevysheva M S Zverev A A Naumova A I Plugina D D Polozhentsev T A Polozhentseva E A Stepanova Tr. Glav. Astron. Obs. Pulkovo, ser. 2 86 4-158 1986 1986TrPul..86....4B Positional data The Catalogue SPF2 was obtained from observations of the fundamental FK4 stars as a reference stars for SRS, BS and DS star. Observations were made by Pulkovo observers in the declination zone -42 to -90 and +16 to -16 degrees using Repsold Meridian Circle of the Cerro Calan Observatory (Santiago, Chile) from 1963 to 1968.
They worked in closed cooperations with their Chilean colleagues who observed other declination zones. In total 15160 observations were made of FK4 stars. The reductions of observations were made by the quasi-absolute method proposed by M.S.Zverev (1969). Investigations were carried out of the systematic differences of type "E-W" as well as of the personal equations. Also differences of type "Upper - Lower culmination" were investigated. All these corrections were applied to the observations. The mean error of the single observations reduced to the equator is +/- 14.0 millisecond of time. The mean error of the position of a single star reduced to the equator is +/- 2.8 millisec of time (each position in the middle are consists from 25 observations). The main results of the systematic errors were published by Zverev and Naumova.
+16 to -16 deg - RA corrections 03 "03" --- ID FK4 number --- mag Magnitude mag RAh Right Ascension (B1950.0) hours h RAm Right Ascension (B1950.0) minutes min RAs Right Ascension (B1950.0) seconds s DE- Declination (B1950.0) sign --- DEd Declination (B1950.0) degrees deg DEm Declination (B1950.0) arcminutes arcmin DEs Declination (B1950.0) arcsec arcsec del_RA RA-RA(FK4) s Ep Epoch of mean observation - 1900 years a e Error E*cos(DE) where E = error of observations s N Number of observations --- -40 to -90 deg - RA and Dec. for 280 stars rem Remark "-3" data of spf2b.dat exist "03" data of spf2b.dat do not exist --- ID FK4 number --- mag Magnitude mag RAh Right Ascension (B1950.0) hours h RAm Right Ascension (B1950.0) minutes min RAs Right Ascension (B1950.0) seconds s DE- Declination (B1950.0) sign --- DEd Declination (B1950.0) degrees deg DEm Declination (B1950.0) arcminutes arcmin DEs Declination (B1950.0) arcsec arcsec del_RA RA-RA(FK4) s Ep Epoch of mean observation - 1900 years a e Error E*cos(DE) where E = error of observations s N Number of observations --- -40 to -90 deg - RA with upper and lower culmination separate 3 "3" --- ID FK4 number --- mag Magnitude mag RAh Right Ascension (B1950.0) hours h RAm Right Ascension (B1950.0) minutes min DE- Declination (B1950.0) sign --- DEd Declination (B1950.0) degrees deg DEm Declination (B1950.0) arcminutes arcmin uRA RA-RA(FK4) (upper culmination) s uEp Epoch of mean obs (upper culmination) - 1900 a ue Error (upper culmination) s uN Number of observations (upper culmination) --- lRA RA-RA(FK4) (lower culmination) s lEp Epoch of mean obs (lower culmination) - 1900 a le Error (lower culmination) s lN Number of observations --- Nancy Grace Roman and Julie Anne Watko SSDOO/ADC 1996 Feb 29 We appreciate the extensive information provided by D. Polojentsev. I_44.xml AGK3 Catalogue 1061B I/61B AGK3 Catalogue AGK3 Catalogue W Dieckvoss O Heckmann Hamburg-Bergedorf ??? ??? 1975 1975QB6.A15.......D I/176 : AGK3U: an updated version of the AGK3 (Bucciarelli+ 1992) I/69 : AGK3 Catalogue by Right Ascension (Dieckvoss, Heckmann 1975) I/161 : AGK3R (Smith 1990) Cannon, A. J. (1925-1936), The Henry Draper Extension, Ann. Astron. Obs. Harvard College 100. Cannon, A. J. and Pickering, E. C. (1918-1924), The Henry Draper Catalogue, Ann. Astron. Obs. Harvard College 91-99. Dieckvoss, W. (in collaboration with H. Kox, A. Gunther and E. Brosterhus) (1975), AGK3 Star Catalogue of Positions and Proper Motions North of -2.5 Degrees Declination, Hamburg-Bergedorf. Nagy, T. A. 1979, Documentation for the Machine-Readable Version of the AGK3 Catalogue of Positions and Proper Motions North of -2.5 Degrees Declination, Systems and Applied Sciences Corporation R-SAW-7/79-35. Warren, W. H. Jr. and Kress, K. 1980, Astron. Data Center Bull. 1, 19. Willstrop, R. V. 1983, Bull. Inf. Cent. Donnees Stellaires No. 24, 65. Positional data Proper motions Magnitudes, photographic The AGK3 provides positions and proper motions for stars north of -2.5 degrees. For the most part, it contains the stars in the AGK2 but is based on newly remeasured reference stars whose positions were reduced to the FK4 system. A list of 446 AGK2 stars not in the AGK3 and of three new stars is provided. All plates were taken at the Bergedorf Observatory. In addition to the positions and proper motions, the catalog contains magnitudes and spectral types, the epoch of the observations, the epoch difference between the AGK2 and AGK3, and the BD numbers.
The AGK3 Star Catalogue of Positions and Proper Motions North of -2.5 Degrees Declination (hereinafter AGK3) was conceived and planned during discussions between O. Heckmann and D. Brouwer at Hamburg Observatory following the 1952 International Astronomical Union (IAU) General Assembly in Rome. It was concluded that an adequate number of reference stars (AGK3R) should be observed by as many meridian circles of as many observatories as possible, the revision of FK3, then in progress (FK4), should define the reference frame, and the same instruments as used for AGK2 should be used for the observations for AGK3. A formal recommendation was adopted through Commission 8 at the 1955 IAU General Assembly in Dublin, with the observatories at Babelsberg, Bergedorf, Bordeaux, Greenwich, Heidelberg, Nikolajew, Ottawa, Paris, Pulkovo, Strasbourg and Washington (USNO) to collaborate in the work, and with F. P. Scott (USNO) to coordinate the meridian circle observations of AGK3R stars. The completion of the photographic observations was to be the responsibility of the observatories at Bergedorf and Bonn, with all plate measurements to be done at the former. (However, it was finally decided that all plates, even for the AGK2 Bonn zones, would be taken at Bergedorf.) The plates for AGK3 were secured at Bergedorf between August 1956 and June 1964, with special precautions (exposures on both sides of the pier) made to compensate for possible changes in the camera objective. The two sets of plates were measured at Bergedorf in opposite directions and averaged to obtain final x,y coordinates. The detailed procedures for the correction of magnitude-color errors, reduction of the measures using the AGK3R stars, re-reduction of AGK2 using its reference catalog AGK2A transformed to the FK4 system, and final reduction of the AGK3 positions and proper motions, are discussed by W. Dieckvoss in his technical introduction to the source reference. Although a more detailed discussion of errors is given by Dieckvoss, the standard error for one coordinate on one plate as determined from a limited sample of 110 pairs of plates is +/- 0.025" for AGK3.
Catalog Data AGsign Sign of AGK3 number. --- AGzone AGK3 zone. --- AGnum AGK3 number AGK3 number in increasing order within each declination zone. The field is filled with preceding zeros. --- m_AGnum Component for duplicates Component identification where duplicates AGK3 numbers occur. The lower case letters "a" and "b" may be present. --- Pmag Photographic magnitude from AGK2 mag Sp Spectral type Spectral Type from Henry Draper Catalogue (Cannon and Pickering, 1918-1924), its Extension (Cannon, 1925-1936), Schildt (Yale Transactions) or determined by A. N. Vyssotsky and collaborators at the Leander-McCormick Obs. --- RAh Right ascension hours (1950.0) h RAm Right ascension minutes (1950.0) min RAs Right ascension seconds s DE- Sign of declination (1950.0) --- DEd Declination degrees (1950.0) deg DEm Declination minutes arcmin DEs Declination seconds arcsec nobs Number of photographic observations Number of photographic observations used to determine the position. Single-digit numbers are preceded by a zero. --- Ep-1900 Epoch of AGK3 position minus 1900 yr pmRA Annual proper motion in right ascension Annual proper motion in right ascension multiplied by cos(delta), determined by differencing the AGK3 and AGK2 positions and dividing by the epoch difference. Proper motions are missing for stars new in AGK3 (see Table 6). If a calculated value of the proper motion exceeded the field capacity a value of "9999" is given with a "+" in byte 38. The suggested format reads the datum in the correct units. mas/yr pmDE Annual proper motion in declination mas/yr dEpoch Epoch difference AGK3-AGK2 yr BD Full BD catalog designation The full BD identification (see cat. <I/122>) contains: bytes 59-60: "BD" or blank byte 61: Sign of BD zone number bytes 62-63: BD zone number bytes 64-68: BD number within zone --- m_BD Component of multiple system Numerical code for identification of a component of a multiple system: (1 = primary [P]; 2 = secondary [S]; 3 = A; 4 = B; 5 = S1; 6 = S2; 7 = P1; 8 = P2; 9 = C). BD supplemental stars (lower case letters) are assigned codes but are indistinguishable from A and B designations because the codes are the same. Since the file format only allows one byte for the duplicity code, and nine codes are already used, the distinction cannot be drawn. If it is necessary to distinguish or identify supplemental stars, the Catalog of BD Supplemental Stars (Warren and Kress 1980) should be used. --- Sum Sum of discrepancy codes Sum of discrepancy codes, calculated as the sum of 2**v (2 to the power of v), where v = 0 (BD number), 1 (mpg and/or spectral type), 2 (AGK2 right ascension), 3 (AGK2 declination), 4 (AGK3 right ascension), 5 (AGK3 declination). --- pmsec Annual proper motion in seconds of RA, computed by dividing by 15cos(delta) s/yr dRA The difference in right ascension in the sense AGK3 - AGK2modified The residual quantity of the difference in right ascension (multiplied by cos(delta)) in the sense AGK3 - (AGK2modified), where the last quantity denotes data from the re-reduced AGK2. arcsec dDE The difference in declination in the sense AGK3 - AGK2modified arcsec agk3.doc Documentation James E. Gass and Gail L. Schneider SSDOO/ADC 1997 Jul 01 UNKNOWN UNKNOWN The machine version of the AGK3 was received on magnetic tape from the Centre de Donnees Stellaires, Strasbourg in 1978. The version received had been obtained originally from the Astronomisches Rechen- Institut in Heidelberg. A preliminary document for a modified and corrected version of the catalog was produced by Nagy (1979). The following changes were made to the Heidelberg file in order to correct some minor errors and to produce a file conforming more closely to the published version: 1. AGK3 component identifications for stars where more than one AGK3 star has the same number were changed from upper case characters (A, B) to lower case (a, b) as in the printed edition. 2. Nine stars in AGK3 zone -00, but in BD zone +00 were found to have a BD zone of +90. The BD zone for these stars was changed to +00. These stars are: AGK3 -00 1467, 1510, 1530, 1531, 1532, 1602, 1693, 1774, and 2120. 1-Jul-1997: Explicit decimal points added to floating point fields in computer-readable version. Document brought up to standard. [J. Gass, ADC] 1-Sep-1998: filled blanks between sign and value with zeroes in columns pmRA, pmDE, pmsec, dRA, dDE to allow correct interpretations [F. Ochsenbien, CDS] I_61B.xml Perth 70: A Catalogue of Positions of 24900 Stars Part B, Mean Values of the Observations 1062C I/62C Perth 70 B: Positions 24900 Stars Perth 70: A Catalogue of Positions of 24900 Stars Part B, Mean Values of the Observations E Hog J von der Heide Abh. der Hamberger Sternwarte, Band IX. ??? ??? 1976 1976AAHam...9....1H Astrometric data Photometry This Perth 70: A Catalogue of Positions of 24900 Stars contains accurate positions and magnitudes of 24,871 reference stars, mostly in the southern hemisphere, plus other useful data such as approximate proper motions, radial velocities, and parallaxes. The Perth 70 is a result of meridian circle observations made by the Hamburg Observatory expedition to Perth as part of the international effort on Southern Reference Stars (SRS). The catalog described here provides the mean values for each star, including the position, magnitude, and mean epoch of observation; the proper motions, however, were neither observed nor recomputed from comparing the Perth positions to older material.
This catalog is the September 1992 version of the results of meridian circle carried out at Perth in the late 1960's and early 1970's. Some 107 circumpolar stars occupy two records each, one for observations at upper culmination and one for observations at lower culmination, so the number of records is greater than the number of stars. This file contains the mean values of the meridian circle observations (position and magnitude) made at Perth, plus auxiliary quantities usually taken from the preliminary version of the Southern Reference Stars (SRS) catalog (Corwin, 1992). The first part of each record presents the same information that is contained in the printed catalog; the remaining information was not printed. Missing data are denoted by blank-filled fields except for the standard errors of one observation in R.A. * cos(dec) and in declination. In those fields, missing data are indicated by "0". Stars with numbers in the 30000's are in the FK4 catalog, with the last four digits being the FK4 number. Stars with numbers in the 40000's are in the Bright Star Catalog in the same format. Stars with other numbers are program stars.
The catalog ID Perth 70 catalog number --- n_ID S means star is in the FK4 suppl. --- V V magnitude If the hundredths place (byte 12) is blank, the number was copied from the preliminary SRS; otherwise, the magnitude was observed at Perth. mag Sp Spectral type; from SRS The spectral types are always those of the printed catalog. Two stars must be mentioned specifically: fl2 Velorum (SRS #30309) and O Cygni (SRS #44262). The first, a Wolf-Rayet star (type WC), is listed in the FK5 as "Oap" (the HD designation) and appears here as "O0." The second, a Mira Ceti-type pulsating variable, spectral type "S7ev," appears here as "M7." --- RAh Right ascension hours (B1950) Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. h RAm Right ascension minutes (B1950) Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. min RAs Right ascension minutes (B1950) Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. s cul Culmination flag This is blank except for circumpolar stars, which have 2 records, one marked `U' for upper culmination observations, and one marked `L' for lower culmination observations. --- DE- Sign of declination --- DEd Declination degrees (B1950) deg DEm Declination minutes (B1950) arcmin DEs Declination seconds (B1950) arcsec epRA Mean epoch of observation in RA -1900000 Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. ma epDE Mean epoch of observation in dec -1900000 ma o_RA Number of observations in RA Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. --- RAdel Indicates >=1 obser. in RA deleted Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. --- o_DE Number of observations in declination --- DEdel Indicates >=1 obser. in dec deleted --- q_RAs Residual in right ascension Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. These are the Perth position minus the position in the preliminary SRS, corrected for proper motion to the mean epoch of observation. The signs of the residuals are changed for circumpolar stars observed at lower culmination. carcsec q_DEs Residual in declination carcsec pmRA Proper motion in right ascension Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. These are copied from the preliminary SRS; the Perth 70 positions were not used to compute them. For centennial proper motions, use formats F7.3 and F7.2 for proper motion in RA and proper motion in declination, respectively. s-5/a pmDE Proper motion in declination These are copied from the preliminary SRS; the Perth 70 positions were not used to compute them. For centennial proper motions, use formats F7.3 and F7.2 for proper motion in RA and proper motion in declination, respectively. arcsec-4/a DMcat Durchmusterung catalog The catalog identifier (bytes 84-85) is either `BD' for Bonner Durchmusterung, `CD' for Cordoba Durchmusterung, or `CP' for Cape Photographic Durchmusterung. The zone is contained in bytes 87-89 (with the sign in byte 87), and the serial number, in bytes 90-94. --- DMzone Durchmusterung zone --- DMnum Durchmusterung number --- type Type of star One of `P' for program star, `F' for FK4 star, or `B' for Bright Star Catalog star. --- obs_no Observing number for part A This number is included to enable cross references between this catalog and Part A; it does not appear in the printed catalog and should not be used as the principal identification number. Circumpolar stars have distinct observing numbers for upper and lower culmination. (Part A lists the individual observations.) --- o_obs_no Number of records in part A --- n_n_ID FK4 Supplement number --- RV Radial Velocity dkm/s Plx Parallax marcsec o_V Number of observations of magnitude --- n_V Indicates >=1 obser. in V deleted --- mean Mean epoch of observation in V -190000 ca e_RAs Standard error of one obs. in RA*cos(dec) Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. carcsec e_DEs Standard error of one obs. in declination carcsec e_V Standard error of one obs. in magnitude cmag n_PlxRA Mean parallax factor in right ascension Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. carcsec n_PlxDE Mean parallax factor in declination carcsec pre_V V magnitude from preliminary SRS cat. The preliminary SRS positions may be recovered by RA SRS =RA Perth-PM RA(t RA-1950)+/-(delta RA cos(dec))=15cos(dec SRS) dec SRS = dec Perth-PM dec(t dec-1950)+/-delta dec where t is the mean epoch for the coordinate. The plus sign is taken only for stars observed at lower culmination. The factor 15 in the first equation emphasizes that ff cosffi is tabulated in arc seconds whereas right ascension is customarily expressed in units of time. mag newperth.doc The original more detailed ADC document N. G. Roman SSDOO/ADC 1997 May 27 I_62C.xml Positions and proper motions OF 1981 stars in the vicinity of {alpha} Per 1068A I/68A Positions and Proper Motions in alpha Per cluster Positions and proper motions OF 1981 stars in the vicinity of {alpha} Per A Fresneau Bull. Inform. CDS 18 81 1980 1980BICDS..18...81F Positional data Proper motions Regional catalog A list of positions and proper motions is given for 2027 stars of magnitude 7.5 to 12.5 within a radius of 3.5 deg. of alpha Persei. The values are poor for stars fainter than 11. The present list supersedes the microfiche edition (catalogue I/68/) which was described in the Bull. Inform. CDS 18, 81 (1980).
alpha Per - Catalogue Mel20 Heckmann's number number as published in Astron. Nachr. 283, 109 (Mitt. Hamburger Sternw. 1956MiHam..10...37H) if the star belongs to Heckmann's list --- BD BD (cat. <I/122>) or CSI (Catalogue of Stellar Identifications) this identification is not in BD when a dash (-) follows the degree zone number. --- SpType Spectral type (from Heckmann) --- Pmag Photographic Magnitude, in 0.1 magnitude 0.1mag Epoch Epoch of equatorial coordinates yr RAh RA 1950 at Epoch (hours, always 3) h RAm RA 1950 at Epoch (minutes) min RAs RA 1950 at Epoch (seconds) s e_RAs Mean error on RA (seconds) a zero mean error means that only one observation is available, and hence the mean error is undefined. s pmRA Proper motion mu_alpha in time seconds/century s/ha e_pmRA Mean error on pmRA s/ha DE- Declination 1950 at Epoch (sign) --- DEd Declination 1950 at Epoch (Degrees) deg DEm Declination 1950 at Epoch (Arc minutes) arcmin DEs Declination 1950 at Epoch (Arc seconds) arcsec e_DEs Mean error on Dec (arc seconds) arcsec pmDE Proper motion mu_delta in arcsec/century arcsec/ha e_pmDE Mean error on pmDE arcsec/ha Alain Fresneau, Francois Ochsenbein Strasbg Obs. 1993 Mar 26 I_68A.xml AGK3 Catalogue 1069 I/69 AGK3 Catalogue by Right Ascension AGK3 Catalogue W Dieckvoss O Heckmann Hamburg-Bergedorf ??? ??? 1975 1975QB6.A15........ Positional data Proper motions Magnitudes, photographic The AGK3 catalog of positions and proper motions is a photographic catalog based on plates taken with the same instruments as the AGK2 and referred to a network of meridian observations (the AGK3R). The AGK2 positions were rereduced using its reference catalog, AGK2A, reduced to the FK4 system. The positions and motions are on the FK4 system. The positional errors in one coordinate are about 0.025". Information contained in the catalog includes in addition to the positions and proper motions in the B1950 system, the AGK3 zone and number, a component identification when duplicate AGK3 numbers occur, photographic magnitude, spectral type, number of photographic observations used to determine the position, epoch of the position, epoch difference: AGK3 - AGK2 and the DM number and component.
Data AGK- Sign of AGK3 number. --- ZONE AGK3 declination zone. --- ID AGK3 number in order within zone. --- DUP Component id for duplicate numbers. number=1 The lower case letters "a" and "b" may be present if there are multiple components, otherwise there is a "0". --- mpg Photographic magnitude. number=2 Taken from AGK2. mag Sp Spectral type. number=3 Adopted from the Henry Draper Catalogue (Cannon and Pickering 1918-1924), its Extension (Cannon 1925-1936), Schildt (Yale Transactions) or determined by A. N. Vyssotsky and collaborators at the Leander-McCormick Obs. --- RAh Right ascension (hours) (Equinox 1950.0). h RAm Right ascension (minutes) min RAs Right ascension (seconds) s DE- Sign of declination (Equinox 1950.0). --- DEd Declination (degrees) deg DEm Declination (arcminutes) arcmin DEs Declination (arcseconds) arcsec Num Number of photographic observations used to determine the position. --- Epoch Epoch of AGK3 position - 1900. a pmRA- Sign of proper motion in right ascension. --- pmRA Proper motion in right ascension. number=4 Multiplied by cos(DEC), determined by differencing the AGK3 and AGK2 positions and dividing by the epoch difference. Proper motions are missing for stars new in AGK3 (see Table 6). If a calculated value of the proper motion exceeded the field capacity a value of "9.999" is given with a "+" in byte 38. arcsec/a pmDE- Sign proper motion in declination. --- pmDE Proper motion in declination. number=4 Multiplied by cos(DEC), determined by differencing the AGK3 and AGK2 positions and dividing by the epoch difference. Proper motions are missing for stars new in AGK3 (see Table 6). If a calculated value of the proper motion exceeded the field capacity a value of "9.999" is given with a "+" in byte 38. arcsec/a SepEp Epoch difference AGK3-AGK2. a BD- Sign of zone number --- BD BD catalog designation --- BDZONE BD zone. --- BDNum BD number within zone. --- pmRAt- Sign of right ascension proper motion. --- pmRAt Proper motion in right ascension. number=5 In units of seconds of time per year. Computed by dividing by 15cos(delta). s/a d(RAmod)- Sign of right ascension difference. --- d(RAmod) Residual quantity of the difference. number=6 Residual in right ascension (multiplied by cos(delta)) in the sense AGK3 - (AGK2modified), where the last quantity denotes data from the re-reduced AGK2. arcsec d(DEmod)- Sign of declination difference. --- d(DEmod) Residual quantity of the difference. number=7 Residual in declination in the sense AGK3 - (AGK2modified). arcsec agk3_ra.doc Original ADC documentation Edward J. Shaya SSDOO/ADC 1997 Jul 15 I_69.xml Catalog of Supplemental Stars to the Bonner Durchmusterung 1071 I/71 Bonner Durchmusterung Supplemental Stars Catalog of Supplemental Stars to the Bonner Durchmusterung W H Warren Jr. K Kress unpublished ??? ??? 1980 1980 Durchmusterungen The Bonner Durchmusterung catalogs (Argelander 1859-62, Kuestner 1903), declination zones +89deg. to -01deg., contain supplemental stars having lower case letter designations following the BD numbers after which they have been inserted. Many problems of identification have arisen over the years because the supplemental stars have been included in certain machine-readable catalogs without their letter designations, thus making it impossible for a computer to distinguish between a BD star and its insert(s). The need for a machine-readable version of the supplemental stars arose in connection with identifying stars in other catalogs in order to add the letter designations to them. The initial catalog of supplemental stars was prepared from the second edition of the BD (Kuestner 1903), but proofreading and checking were accomplished by using the reprinted edition (Bonn Universitaets Sternwarte 1968) which incorporated all errata known at that time. In that way, it was possible to simultaneously derive tables of supplemental stars added, deleted, or modified for the reprinted edition. The machine-readable version of the Catalog of Supplemental Stars to the Bonner Durchmusterung is a compilation of Bonner Durchmusterung stars having lower case letter designations in the original published edition of the catalog. The data include all information given in the original published edition as footnotes except for the old spectral types sometimes reported there.
The catalog BDs BD number sign --- BDz BD zone --- BDno BD number within zone BD numbers are determined by the position of the footnoted star in the original published catalog. --- let Letter designation --- RAh Right ascens.(1855)hours Equinox 1855. h RAm Right ascen.(1855)min Equinox 1855. min RAs Right ascen.(1855)sec Equinox 1855. 0.1s RAds Right ascen.(1855)decisec Equinox 1855. ds DE- Sign of declination (1855) --- DEd Declination (1855) degrees deg DEm Declination (1855) minutes 0.1arcmin DEdm Declination (1855) decimin darcmin mag Magnitude Magnitudes are visual and were taken directly from the published catalog. mag Nancy G. Roman ADC/SSDOO 1995 Jun 13 The original document for this catalog was prepared in Script by Wayne H. Warren Jr. It was translated to ASCII and put into the current standard form by the undersigned. The only other change was to fill blanks in the position coordinates with zeros to facilitate proper reading. UNKNOWN UNKNOWN The original BD supplemental data were transferred to coded forms by K. Kress at the National Space Science Data Center (NSSDC), NASA Goddard Space Flight Center. They were also transferred to punched cards at NSSDC, and thence to a computer disk file accessible via an interactive system. The listed file was then proofread against the reprinted microversion (Bonn Universitaets Sternwarte 1968) and additions, deletions, and modifications were made to the file by W. H. Warren Jr. All letter designations are coded as lower case characters just as they appear in the original published catalog. The order of the stars in the catalog is from north to south and increasing right ascension within each declination zone. The magnitude data must be read in character format because the words VAR and NOV occur within the field and byte 27 contains a ? in one case. Tables 1-3 list stars that were either added, deleted, or had their designations changed in the 1968 reprinted edition of the BD. These lists enable the user to resolve differences between this catalog of supplemental stars and the 1903 edition of the published catalog, which is much more widely available than the 1968 edition. Table 1 Stars Added in Reprinted Edition ------------------------------------------------------------------------------- -00 2281a +26 1414a +35 180a +42 3093a +45 3139a +48 3799a -00 3110a +26 2056a +36 4154a +42 4100a +45 3141a +49 80a -00 4212a +26 2059a +37 3418a +42 4178a +46 489a +49 937a +00 4718a +28 258a +39 4869a +42 4611a +46 499a +49 1405a +02 2309a +28 1280a +40 260a +43 1164a +46 2755a +49 1571a +03 1727a +28 4536a +40 2004a +43 1784a +46 2844a +49 2117a +04 2289a +29 3503a +40 2006a +43 2563a +46 2886a +49 3452a +04 3561a +29 4240a +40 3209a +43 3248a +46 2912a +49 3546a +05 462a +29 4470a +40 4729a +43 3913a +46 3116a +49 4309a +12 206a +30 420a +41 312a +43 4086a +46 3934a +50 242a +15 4266a +30 4456a +41 1607a +43 4119a +47 630a +50 1907a +16 4370a +31 366a +41 1608a +43 4388a +47 1278a +56 606a +17 2116a +31 2042a +41 2269a +44 312a +47 3074a +56 2616a +18 368a +32 4341a +41 2680a +44 1308a +47 3202a +57 2864a +18 3421a +32 4668a +41 2680b +44 2480a +48 1302a +58 764a +19 339a +33 21a +41 3640a +44 2721a +48 1391a +58 1096a +21 1842a +33 1429a +42 376a +44 3419a +48 1538a +59 2826a +21 2355a +33 4238a +42 401a +45 513a +48 1783a +67 1046a +21 3114a +34 527a +42 1084a +45 1068a +48 1986a +76 857a +23 1503a +34 666a +42 1798a +45 1073a +48 2827a +78 314a +26 71a +34 4595a +42 2954a +45 1215a -------------------------------------------------------------------------------- Table 2 Supplemental BD Stars Deleted from Original Edition in Reprinted Edition -------------------------------------------------------------------------------- +13 5168a +15 612a +46 1767a -------------------------------------------------------------------------------- Table 3 Modifications of Original Supplemental Numbers in Reprinted Edition -------------------------------------------------------------------------------- +40 4729a changed to +40 4729b, +40 4729a added +48 1302a changed to +48 1302b, +48 1302a added -------------------------------------------------------------------------------- I_71.xml Catalogue of 20457 Star Positions Obtained by Photography in the Declination Zone -48 to -54 Degrees (1950) 1073B I/73B Sydney Photographic Cat 20457 Stars, -48 to -54 Catalogue of 20457 Star Positions Obtained by Photography in the Declination Zone -48 to -54 Degrees (1950) H Eichhorn W D Googe C F Lukac J K Murphy AJ 88 546 1983 1983AJ.....88..546E Positional data Photographic catalog This catalog is also known as the Sydney Photographic Catalogue -48 to -54 Degrees or SPC and gives positions determined by the plate overlap method from plates taken at the Sydney Observatory in 1964. The catalog was originally planned to fill part of the gap left by the Yale Zone and Cape Photographic Catalogues, although the gap has in the meantime been closed by catalogs prepared at Sydney Observatory (Nicholson 1979, King and Lomb 1983). Data in the catalog include star number (CPD; identifications not complete), source catalog identification (AC zones) and related information, right ascension/declination on the FK4 system (equinox and equator B1950, average epoch 1964.475), photovisual magnitude, and numbers of images and pairs of diffraction spectra used in computing position.
Catalog Data CPDnum Number in Cape Photographic Durchmusterung From Gill and Kapteyn (1897, 1900). The zone sign (always -) is in byte 1, the zone in bytes 2-3, byte 4 is blank, and the number is in bytes 5-9. The identifications are not complete, i.e., existing CPD numbers are not always present. --- Source Source catalog identification A Gill and Hough (1923) B Jackson and Stoy (1955) 1-120 Plates in Cape AC zone -49 deg 121-240 Plates in Cape AC zone -51 deg (Cape 1913-1926) 241-360 Plates in Sydney AC zone -53 deg (Sydney Obs. 1923-1933; see Wood 1971) where each AC zone is covered by 120 plates and 120 or 240 is subtracted to obtain plate numbers in the -51 deg and -53 deg zones, respectively. --- number Star or plate number in the source catalog --- refstar Asterisk (*) means the star served as a reference star. --- RAh Right ascension hours (1950) Given for the mean coordinate system 1950, ostensibly on the system of the FK4, at the average epoch 1964.475 of all plates which provided data. (If higher accuracy epochs are required, Table I of Eichhorn et al. 1983 should be consulted.) h RAm Right ascension minutes (1950) min RAs Right ascension seconds (1950) s DE- Sign of declination (1950) --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin DEs Declination seconds (1950) arcsec Ptm Photovisual magnitude, taken from existing sources. For AC stars, the magnitudes were computed from data given in the AC and are photographic. Magnitudes are neither precise nor accurate and are given for reference purposes only. mag o_image Number of measured central images used to calculate the published position. --- o_spect Number of pairs of diffraction spectra used to calculate the published position. The number of individual images measured for computing a published position is the number in byte 51 plus twice the number in byte 53 (see Eichhorn et al. 1983). --- adc.doc ADC Documentation James E. Gass SSDOO/ADC 1997 Jul 31 Appreciation is expressed to Dr. H. Eichhorn for providing the SPC on tape and for reviewing and commenting on the original ADC document. UNKNOWN UNKNOWN The machine-readable version of the SPC was received on magnetic tape from records with bytes 1-25 blank and many other blanks throughout the records. The records on this tape had been designed specifically for printing the catalog and microfiching rather than for efficient storage and computing. To increase storage efficiency the following modifications were made after checking with the first author to be certain that the changes would be acceptable. 1. Superfluous blanks were removed from throughout the data records, except for a single separator blank between each of the data fields decreasing the logical record length from 104 to 53 bytes. 2. Leading zeros were added to all right ascension and declination fields. I_73B.xml Third Santiago-Pulkovo Fundamental Stars Catalogue (SPF3) 1078 I/78 SPF3 Catalogue Third Santiago-Pulkovo Fundamental Stars Catalogue (SPF3) P R Loyola V N Shishkina Publ. Dept. Astronomy Univ. of Chile 2 159 1974 1974PDAUC...2..159L I/82 : SPF1 Catalogue (Anguita et al., 1975, =1975PDAUC...2..181L) I/44 : SPF2 Catalogue (unpublished) Fricke, W. and Kopff, A., 1963, Fourth Fundamental Katalog (FK4), Veroeff. Astron. Rechen-Inst. Heidelberg, No. 10. (Catalogue: I/143) Morgan, H.R., 1952, "Catalog of 5,268 Standard Stars for the Equinox and Epoch 1950.0 Based on the Normal System N30", Astron. Papers Amer. Ephemeris 13, Part III. (Catalogue: I/13) Meridian observations Positional data Stars, fundamental The "Third Santiago-Pulkovo Fundamental Stars Catalogue (SPF3)" is a catalogue of right ascensions (the primary datum) of 671 fundamental bright stars, as measured with a Zeiss broken transit instrument at Cerro Calan Observatory in Chile. The observations were made in series consisting of 70 stars observed along the meridian from +42deg to the pole in upper culmination and from the pole to -70deg in lower culmination; the program consisted of 231 series of observations. In addition to the final reduced right ascensions for the program stars, the catalogue contains cross identifications to the N30 (Morgan 1952) and FK4 (Fricke et al. 1963) catalogues, visual magnitudes, approximate declinations (equinox 1950.0), mean epochs of the observations, and mean errors of the determined right ascensions. This document describes the machine-readable version of the SPF3 catalogue as distributed by the Astronomical Data Centers. It is intended to enable users to read and process the catalogue data without unnecessary problems and guesswork. The source reference should be consulted for details regarding the instrument characteristics, measurements, reductions, and comparisons with other catalogues.
The SPF3 Catalogue SPF3 sequential number. --- FK4 FK4 (Fricke et al., 1963) --- N30/GC N30 or GC number (see byte 13). --- n_N30/GC Asterisk (*) if the N30/GC contains a GC identification; otherwise blank. --- Vmag Visual magnitude 0.01mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAms Right Ascension 1950 (milli-seconds) ms DE- Approximate Declination 1950 (sign) --- DEd Approximate Declination 1950 (degrees) deg DEdm Approximate Declination 1950 (deci-minutes) 0.1arcmin EpRA Mean epoch for right ascension observations 0.01yr o_RAms Number of observations --- e_RAms Mean error of RAms ms Dimitri Polojentsev Pulkovo Francois Ochsenbein CDS 1995 Sep 18 Appreciation is expressed to Dr. A. Gutirrez-Moreno of the Universidad de Chile for supplying the published catalogue in printed form, and to M.H. Warren for proofreading the machine-readable version. UNKNOWN UNKNOWN * May 1982: The SPF3 catalogue was keyed directly to disk storage and proofread at the Astronomical Data Center, NASA Goddard Space Flight Center. File documented by Wayne H. Warren Jr., as document NSSDC/WDC-A-R&S 82-17 * 18-Sep-1995: documented with CDS standards; transformed epochs initially starting at 1950.00 I_78.xml Lowell Proper Motion Survey: 8991 Stars with m > 8, PM > 0.26"/year in the Northern Hemisphere 1079 I/79 Lowell Proper Motion Survey 8991 Northern Stars Lowell Proper Motion Survey: 8991 Stars with m > 8, PM > 0.26"/year in the Northern Hemisphere H L Giclas R Burnham Jr. N G Thomas Lowell Obs., Flagstaff, AZ ??? ??? 1971 1971lpms.book.....G I/112 : Southern Hemisphere Lowell Proper Motion Catalog (Giclas+ 1978) Giclas, H. L. 1958, Lowell Obs. Bull. 4, 1 (No. 89). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1961, Lowell Obs. Bull. 5, 61 (No. 112). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1963, Lowell Obs. Bull. 6, 1 (No. 120). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1964, Lowell Obs. Bull. 6, 103 (No. 122). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1964, Lowell Obs. Bull. 6, 135 (No. 124). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1965, Lowell Obs. Bull. 6, 197 (No. 129). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1966, Lowell Obs. Bull. 6, 233 (No. 132). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1966, Lowell Obs. Bull. 6, 271 (No. 136). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1967, Lowell Obs. Bull. 7, 1 (No. 138). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1967, Lowell Obs. Bull. 7, 31 (No. 140). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1968, Lowell Obs. Bull. 7, 67 (No. 144). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1969, Lowell Obs. Bull. 7, 129 (No. 150). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1970, Lowell Obs. Bull. 7, 149 (No. 151). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1970, Lowell Obs. Bull. 7, 165, (No. 152). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1971, Lowell Proper Motion Survey, Northern Hemisphere, The G Numbered Stars (Flagstaff: Lowell Observatory). Giclas, H. L., Slaughter, C. D. and Burnham, R. Jr 1959, Lowell Obs. Bull. 4, 136 (No. 102). Positional data Proper motions The catalog contains a summary of many individual papers published in the Lowell Observatory Bulletins in the years 1958 to 1970. The data in the machine-readable version include observed positions, proper motions, estimated photographic magnitudes and colors, and references to identifications in other catalogs. Photoelectric data on the UBV system are included for many stars, but no attempt was made to find all existing photometry. The notes.dat file was computerized at the ADC by keying the notes directly to disk storage.
Catalog Data G Original G number assigned Original G number assigned to the star on the plate region where it was first Found. Stars which were subsequently found on later plates were assigned new G numbers; however, in this catalog all duplicate observations have been combined and averaged with the original G numbers retained. Byte 1 of the field always contains a "G" and byte 5 always always contains a "-". The number in bytes 2-4 is the plate number, while that in bytes 6-8 is the star number on the plate. --- RAh Right ascension 1950 (hours) Epochs are given for plate regions in the original Lowell Bulletin numbers reported in the CHT column of the published catalog. h RAm Right ascension 1950 (minutes) min RAs Right ascension 1950 (seconds) s DE- Sign of declination --- DEd Declination 1950 (degrees) deg DEm Declination arcmin pm Annual proper motion arcsec/yr pmPA The position angle of proper motion PA of proper motion, measured in the normal way from North through East. deg Pmag Estimated photographic magnitude mag col Estimated color class Color class is on a scale of -1 (bluest) to +4 (reddest). Almost all stars having color class -1 have subsequently been classified as white dwarfs. An approximate relationship between estimated color and UBV colors is given in the published catalog. --- o_pm Number of observations Observations from different plate regions contained in the mean. A value of unity denotes a single observation from one plate pair. Actually, there are never as many as ten observations, so byte 33 is always blank. --- osource Or equivalent References for other sources containing information and/or data about the star. References are separated by blank characters and consist mainly of designations in other catalogs. A symbol "+" following the last reference indicates additional references in the notes to the catalog. The reference key is given in table2.txt. --- flag '*' indicates a note in file notes.dat Note in the published catalog which gives additional information about the star. See notes.dat for a description of the machine-readable notes. --- code Parallax Code Indicates if the star is on a parallax program of some observatory, thus denoting the possibility that a trigonometric parallax may eventually be be available. The following codes are employed: A Allegheny Obs. L Lick M Leander McCormick N U.S. Naval S Sproul V Van Vleck Y Yerkes A digit of >= 2 (= n) indicates the star to be on the working lists of n observatories. The codes for the n observatories are listed in table3.txt. --- Vmag Photoelectric V magnitude Photoelectric V magnitude obtained from the source given in bytes 95-97. UBV data are given for reference purposes only and no attempt for completeness has been made. Blank if no data reported. mag B-V B-V color (blank if no data) mag U-B U-B color (blank if no data) mag r_Vmag Ref code for the magnitude source The magnitude source reference key is given below. A digit >= 2 denotes multiple references (given in the notes.dat). Note: the appended minus signs on some codes are not explained in the published catalog. Lowell Proper Motion Survey, Northern Hemisphere. Magnitude Source Reference Key E1 Eggen, O. J. 1963, Astron. J. 68. 483. E2 Eggen, O. J. 1966, Royal Obs. Bull. No. 120. E3 Eggen, O. J. 1968, Astrophys. J. Suppl. 16, 97 (No. 143). E4 Eggen, O. J. 1969, Astrophys. J. Suppl. 19, 31 (No. 168). E5 Eggen, O. J. 1968, Astrophys. J. 153, 195. EG1 Eggen, O. J. and Greenstein, J. L. 1965, Astrophys. J. 141, 83. EG2 Eggen, O. J. and Greenstein, J. L. 1965, Astrophys. J. 142, 925. EG3 Eggen, O. J. and Greenstein, J. L. 1967, Astrophys. J. 150, 927. ES Eggen, O. J. and Sandage, A. 1967, Astrophys. J. 148, 911. G1 Greenstein, J. L. 1969, Astrophys. J. 158, 281. S1 Sandage, A. 1964, Astrophys. J. 139, 442. S2 Sandage, A. 1969, Astrophys. J. 158, 1115. SK Sandage, A. and Kowal, C. 1962, private communications. WG Gliese W. 1969, Catalogue of Nearby Stars, Veroff. Astron. Rechen-Inst. Heidelberg, No. 22. WA Wanner, J. F. 1964, Ph.D. Thesis, Harvard University. --- Notes G G Star number, as in table north.dat --- m_G Shared note As described for bytes 1-8 in catalog.dat. If more than one consecutive G number is referred to, a slash (/) appears in byte 9 and the final digit of the second G number is given in byte 10. If more than two consecutive G numbers are included, a hyphen appears in byte 9 and the final digit of the last number in byte 10. A comma is given in byte 9 if two non-consecutive G numbers are referenced. Bytes 9 and 10 may also contain component identifications for double stars having the same G number, e.g. "AB". --- count Line counter Used to sequentially number remarks for the same star(s). Can be used as a secondary sort field to reorder the notes properly if they become disorganized. --- Text Text of remark --- table2.txt Key to reference abbreviations table3.txt Supplementary parallax codes Melissa C. Larkin SSDOO/ADC 1997 Mar 10 The original ADC documentation (1983) by Wayne H. Warren, Jr. was used to create this ReadMe file. He also did the original data reformatting. UNKNOWN UNKNOWN The first record in catalog.dat, containing only the word "MUCAT", was deleted. Multiple 80-byte records were combined while deleting a test digit in byte 80 indicating an additional record, and redundant G numbers on multiple records were removed. The machine-readable catalog contains 8989 records. A count of the stars in the published catalog (113 full pages with 75 stars per page and 68 stars on last page) gives 8993; however, stars are missing on pages 28, 29 and 42, resulting in 8989 stars total. Preceding zeroes were added to the G numbers to match the published catalog. There was no distinction between blank and 0.00 color indices. Initially, all zeroes were converted to blanks for B-V and U-B, then the published catalog was scanned for valid 0.00 values and the values were added for the appropriate stars. Plus signs were added to the declinations (byte 15), the color class positive values, and to all positive color indices. The following miscellaneous corrections to the published catalog were made to the machine file: G066-036 photoelectric data deleted as per published version G213-017 Declination degrees corrected from +39 to +37 G128-032 added BD+32 4584-5 The notes file was prepared by keying the published remarks directly to disk and adding to the catalog as a second file. I_79.xml Catalog of 5,268 Standard Stars Based on the Normal System N30 1080 I/80 Catalog of 5268 Standard Stars, Normal System N30 Catalog of 5,268 Standard Stars Based on the Normal System N30 H R Morgan Astron. Papers Amer. Ephemeris 13, Part III ??? ??? 1952 1952N30...C......0M Positional data Proper motions Stars, fundamental Fundamental catalog The catalog was constructed primarily to assist in the reduction and interpretation of planetary observations, particularly those made in the nineteenth century. The new catalog was considered necessary because the only fundamental catalogs available at the time (FK3, GC) have mean epochs around 1900, and over the period of approximately fifty years, positional accuracies had deteriorated from cumulative effects of proper motion inaccuracies. The ADC version of the data file was prepared from the original file by reformatting and incorporating changes to effect uniformity in the data fields. The notes file was created at the ADC by keying the information directly to disk storage. Cross checks were performed to assure that all stars flagged as having notes have entries in the notes file and that all notes are flagged in the data file.
The N30 catalog of 5268 standard stars ID N30 running number --- DMsign DM sign --- DMzone DM zone --- DM DM number (Present for all stars) --- GC GC number (blank if not present) --- HarvaP Harvard photometric magnitude For double stars, if the position is for one component, the magnitude of that component is given and the magnitude, distance and position angle of the companion are given in the notes (remarks.dat). If the position is for the mean, center of light, or center of gravity, the combined magnitude is given and the magnitudes, distance and position angle of the components are given in the notes. Where the position is for the center of gravity, the orbital corrections used in the reduction of the observation were taken from the GC, Vol. I, Ap. II. For double stars of distances 1" to 2", there is an uncertainty as to part observed, depending upon the relative magnitudes of the components. If the components are separated and differ considerably in magnitude, then the use of screens cuts out the fainter star. There are a number of such stars and in older work the observations were reduced as the mean, or center of light. Where it seems probable that the new position is for the brighter star and the GC gives a mean, a note is given. The magnitudes of variable stars are given as a blank followed by three zeroes. 0.01mag HDSp Henry Draper (HD) spectral type Composite spectra are given as combinations; e.g. KOAO or KO+A. A few peculiar composite spectra require > 4 characters and the p's are omitted in the fields, but given in the notes. --- RAh Right ascension (equinox B1950.0) in hours Right ascension for equinox and epoch 1950.0 were brought up from epoch of observation using Newcomb's precession and the proper motions in this catalog. h RAm RA in minutes min RAs RA in seconds s RA3rd Third term in right ascension The first and second terms are not included on the original tape. 0.01s pmRA Centennial proper motion in RA 0.01s/ha v(pmRA) Centennial secular variation in pmRA 0.01s/ha mEpRA Mean epoch of RA (0.1 yr) (1900+) 0.1yr w_mEpRA weight of RA Sum of combining weights used in forming the normal position in RA. --- DE- sign --- DEd Declination (equinox 1950.0) in degrees deg DEm DEC in arcminutes arcmin DEs DEC in arcseconds arcsec DEC3rd Third term in declination 0.1arcsec pmDE Centennial proper motion in declination marcsec/a D(pmDE) Centennial secular variation in pmDE marcsec/a mEpDE Mean epoch of DEC (0.1 yr) (1900+) 0.1yr w_mEpDE weight of DEC Sum of combining weights used in forming the normal position in Dec. --- rem "*" if there is a remark in remarks.dat --- Remarks ID N30 running number --- Dot A period (.) --- rem Remark(s) --- M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1996 Mar 08 The original ADC documentation by Wayne H. Warren, Jr. (1981) was used to create this ReadMe file. He also did the reformatting discussed above. UNKNOWN UNKNOWN The catalog was received on magnetic tape from the Centre de Donnees Stellaires de Strasbourg. The following modifications were made to the format in order to make the records appear more similar to the published catalog, to make them easier to read when listed, and to simplify processing to produce printed and microform versions closely approximating the published catalog in appearance: 1. Data were read and rewritten to discard leading zeroes, which make the numbers difficult to read when listed. 2. All positive Durchmusterung numbers had zeroes in the zone numbers where + signs would ordinarily be. The zeroes were changed to + signs. 3. The GC numbers and secular variations in R.A. and Dec. were changed to blank fields if not present. They were zeroes on the tape as received. 4. Several modifications were made to the spectral types: (a) Peculiar and emission symbols (p, e) were changed to lower case to conform to standard usage. (b) Composite spectra are indicated by two spectral types which run together in the 4-byte field. For types of the form K0A, a change was made to the form K0+A. (c) Peculiar HD O-star types were coded numerically; they were decoded by replacing O1 by Ob, O3 by Od, O4 by Oe5, and O0P by Oap. 5. Plus (+) signs were added to the first byte of the declination field where blanks had been previously. 6. The note indicator (byte 88) was an asterisk (*) in many cases, but for more than half of the stars having notes, a peculiar code was found which printed as b on an extended chain printer. Since there should have been no varying note characters, the latter codes were changed to asterisks for uniformity. The notes file was created and added to the machine-readable catalog. Checks were made to ensure that all records containing an * have corresponding notes and vice versa. I_80.xml First Santiago-Pulkovo Fundamental Stars Catalogue (SPF1) 1082 I/82 SPF1 Catalogue First Santiago-Pulkovo Fundamental Stars Catalogue (SPF1) C Anguita G Carrasco P R Loyola V N Bedin A A Naumova D D Polojentsev T A Polojentseva K N Tavastherna M S Zverev Publ. Dept. Astron., Univ. of Chile 2 181 1975 1975PDAUC...2..181A I/44 : SPF2 Catalogue (unpublished) I/78 : SPF3 Catalogue (Loyola and Shishkina, =1974PDAUC...2..159L) Fricke, W. and Ropff, A. 1963, Fourth Fundamental Katalog (FK4J, Veroeff. Astron. Rechen-Inst. Heidelberg, No. 10. Meridian observations Positional data Stars, fundamental The "First Santiago-Pulkovo Fundamental Stars Catalogue (SPF1)" contains right ascension observations of 1043 FK4 stars made during the period 1963 to 1968 with the Repsold Meridian Circle located at Cerro Calan Observatory in Chile. The FK4 stars were observed during series of observations of Southern Reference Stars (SRS) and Bright Stars (BS) international programs. Approximately 30 to 45 FK4 stars were measured during each 2- to 2-1/2-hour series, and included stars observed along the meridian between +41deg and -90deg in upper culmination and from -90deg to -68deg in lower culmination. The lower culmination observations are given in a separate table in the source reference; they are included in the file "lower". This work was made during the observations of the SRS and BS international programmes. These series of fundamental stars were periodically observed on the whole arc of meridian from +40 deg. to -68 sp deg. 211 series of observations were made with 6793 RA of stars observed. The reduction of observations was made by Zverev's quasi-absolute method (M.S.Zverev, Astr.J. USSR, 1965, v.42, p.823 and 1969, v.46, p.129.). The mean error of the positions of stars in the Catalogue is M.E. (Delta Alfa x cos Dec.) = +/- 0.008 timesec.
The SPF1 Catalogue Lower culminations FK4 Number in the FK4 catalogue (Fricke and Kopff 1963). --- RAh Approximate Right Ascension 1950 (hours) h RAm Approximate Right Ascension 1950 (minutes) min DE- Approximate Declination 1950 (sign) --- DEd Approximate Declination 1950 (degrees) deg DEm Approximate Declination 1950 (minutes) arcmin dRAms(i) Correction to the FK4 right ascension in the instrumental system (RA-RA(i)) for the mean epoch of the observations. ms dRAms(FK4) Correction to the FK4 right ascension in the FR4 system for the mean epoch of the observations. ms o_dRAms(i) Number of observations for dRAms(i) --- e_dRAms(i) Mean square error of the catalogue position multiplied by cos(delta), computed with the deviations of the observations from the mean. ms Epoch Mean epoch of the observations yr Dimitri Polojentsev Pulkovo Francois Ochsenbein CDS 1995 Sep 18 Appreciation is expressed to Dr. A. Fresneau of the CDS, Strasbourg, for preparing a handwritten format description of the CDS tape at my request, and to Dr. A. Gutirrez-Moreno for sending the University of Chile publication required for comparison purposes. UNKNOWN UNKNOWN * March 1982: The SPF1 catalogue was received on magnetic tape from the Centre de Donnees Stellaires (CDS), Strasbourg. The data had been received on punched cards from the Astronomisches Rechen-Institut, Heidelberg and had been punched from a handwritten version (A. Fresneau, private communication). A check against the published catalogue (Anguita et al. 1975) revealed an extra record in the machine-readable version (FR4 #1121 with only one observation; the observation must have been removed before publication and has been deleted from the file) and one record having an incorrect FK4 number and displaced (this has been corrected), plus several stars whose right ascensions and declinations disagree by 1m or 1' between the computer file and the published catalogue (these have not been changed since the right ascensions and declinations are only approximate and are not the principal data of the catalogue). The logical record length (LRECL) of the file received (the upper and lower culmination observations were on a single file) was 88 bytes (a card image plus 8-byte allowance for CDS identification number); since bytes 50-88 were always blank, LRECL was changed to 49 bytes to save storage space. The upper and lower culmination tables were separated into two files due to the fact that lower culmination observations are made at lower altitude and are often of lower accuracy than upper culmination observations. * 18-Sep-1995: Documentation standardized at CDS. I_82.xml Cape Photographic Catalogue 2 1085 I/85 Cape Photographic Catalogue 2 Cape Photographic Catalogue 2 W Nicholson M J Penston C A Murray C de Vegt Mon. Not. Roy. Astron. Soc. 208 911 1984 1984MNRAS.208..911N Positional data Proper motions Photographic catalog This catalog contains the provisional positions for 51018 stars in the Cape zone -40 deg. to -52 deg., on the FK4 system for the equinox 1950.0. The internal mean error of a single coordinate obtained from the mean of r=four plates is estimated to be less than +/- 0.1" at the mean epoch of observation, about 1962. The systematic deviation from the FK4 system in a small area is probably also about +/-0.1". New proper motions have been determined for 22731 stars which are also in the Smithsonian Astrophysical Observatory (SAO) catalogue; the formal mean error of an annual proper motion in each coordinate is about +/-0.004"/a.
The usable width of each plate is 4.1 deg. Stars were selected from the SRS and SAO catalogs, with the SRS providing the reference frame. All SAO stars were included except in crowded fields near the galactic plane, in which many SAO stars were omitted. Stars were then added by visual inspection to bring the number up to about 250, with as uniform a distribution as possible over the plate. The number of stars measured per plate varied from 70 to more than 700. The numbering system adopted is based on the South Polar Distance of a band of declination 1 deg. wide with the stars within each band being numbered sequentially in the order of right ascension. Approximate visual magnitudes have been determined from the image diameters calibrated by the V values from the published literature. Only three plates have fewer than 10 such standards; 75% of the plates have between 15 and 30. Generally, the available stars are brighter than V-9.5 mag.
The catalog ID CPC2P number --- SAO SAO number --- SRS SRS number --- RAs Right ascension seconds (1950) s DE- Sign of declination --- DEs Declination seconds (1950) arcsec mag Magnitude cmag ep Epoch of observation - 1900 a e_RAs Internal mean error in RAs arcsec e_DEs Internal mean error in DEs arcsec n_mag Magnitude status 0 = not available 1 = normal 2 = variable --- o_pos Number of plates used for position --- o_mag Number of plates used for magnitude --- del_SS Separation of SRS and CPC2 positions arcsec pmRA Annual proper motion in RA s-4/a pmDE Annual proper motion in declination marcsec/a e_pmRA Mean error of proper motion in RA s-4/a e_pmDE Mean error of pm in declination marcsec/a del_pm Larger pm diff. |CPC2-SAO| in RA or DE marcsec/a N. G. Roman ADC/SSDOO 1997 Jul 25 I_85.xml Sydney Southern Star Catalogue 1086A I/86A Sydney Southern Star Catalogue Sydney Southern Star Catalogue D S King N R Lomb J. Proc. R. Soc. N. S. W. 116 53 1983 1983 Astrometric data Positional data Proper motions This catalogue principally covers the range between -51deg. and -63.5 deg and contains positions and proper motions for 29,926 stars. 3244 faint Astrographic stars were added to supplement the stars at fainter magnitudes. Positions in standard form (hours, minutes, and seconds of time for the right ascensions and degrees, minutes, and seconds of arc for the declinations) have been added to the machine readable version of this catalogue.
The Sydney Southern Star Catalogue contains the results of the Sydney Observatory astrometric program during the two decades ending in 1983. Declination zones centered on -53.5, 58.5, -56.0, -58.5, -61.0, and -63.5 deg. have been measured and are included. The plates were taken with a 23-cm Taylor, Taylor, and Hobson camera and measured with a Grubb-Parsons photoelectric measuring machine. The reference catalogue used was the WL50. The standard error of a position based on four images is 0.10" in either coordinate. A 2.3 magnitude diffraction grating was used to produce side images shifted from the central image in declination. The stars selected were compiled from the Cape Photographic Catalogue for 1950 (CPC) (Jackson and Stoy 1954-1958), International Reference Stars (IRS) (Scott 1962), Cape Zone Cataloge for 1900 (ZC) (Gill and Hough 1923, Spencer Jones and Jackson 1936), Albany General Catalogue (GC) (Boss 1937) and the Sydney Astrographic Catalogue (AC) (Nangle and Wood 1925-1971). The Sydney AC was used to obtain 3244 supplementary faint stars so that about one star per square degree is in the photographic magnitude range 11.0 to 11.5. All of the AC stars were given a magnitude of 12.0 to distinguish them as AC stars although they are presumed to be in the stated photographic magnitude range. In the area south of -63.5 deg., only the IRS stars were selected for measurement. This was to give complete plate coverage for the determination of plate constants for the plates centered at -6358.5 deg. 395 IRS stars are included in this zone. CPC stars and AC stars were selected for measurement between declinations -52deg. and -63.5 deg. Between -51deg. and -52deg., the measuring list was prepared by supplementing the few CPC stars in this area with ZC stars, GC stars, and IRS stars. In general, stars brighter than photographic magnitude 6.0 were excluded and stars brighter than photographic magnitude 8.1 had their first order side images measured as well as the central image, giving three measurements.
Positions and proper motions for 23287 stars num Number --- magpg Photographic magnitude 0.01mag RAh Hours right ascension (1950) h RAm Minutes right ascension (1950) min RAs Seconds right ascension (1950) s DE- Sign of declination --- DEd Degrees declination (1950) deg DEm Minutes declination (1950) arcmin DEs Seconds declination (1950) arcsec RAsec Right ascension in seconds 0.001s DEsec Declination in arcseconds 0.01arcsec Epoch Epoch - 1900.000 0.001yr N No. observations --- pmRA Proper motion in right ascen. 0.0001s/yr pmDE Proper motion in declination 0.001arcsec/yr Positions, only, for 3244 faint stars Positions, only, for 395 stars south of declination -63.5 deg. num Number --- magpg Photographic magnitude 0.01mag RAh Hours right ascension (1950) The positions are for the equinox B1950 and the reference system used was Washington El Leoncito 50. h RAm Minutes right ascension (1950) min RAs Seconds right ascension (1950) s DE- Sign of declination --- DEd Degrees declination (1950) deg DEm Minutes declination (1950) arcmin DEs Seconds declination (1950) arcsec RAsec Right ascension in seconds 0.001s DEsec Declination in arcseconds 0.01arcsec Epoch Epoch - 1900.000 0.001yr N No. observations --- Nancy G. Roman SSDOO/ADC 1995 Mar 28 We thank Dr. Lomb for supplying us with the machine-readable version of the Sydney Southern Star Catalogue and for a preprint of the Source Reference. UNKNOWN UNKNOWN Construction of the current version of the Sydney Southern Star Catalogue The machine-readable file was received on magnetic tape from Dr. N. R. Lomb of the Sydney Observatory in November, 1983 in excellent shape. As received, the catalogue contained two files. The primary catalogue file contained right ascensions and declinations in milliseconds of time and hundreths of a second of arc, respectively. The second file contained the data for both the faint Astrographic stars and the southern IRS stars. In the present version, sexigesimal positions (hours and degrees) have been added in addition to the form given on the tape as received and the Astrographic and IRS data have been divided into separate files. I_86A.xml LHS Catalogue: a catalogue of stars with proper motions exceeding 0.5" annually. 1087B I/87B LHS Catalogue, 2nd Edition LHS Catalogue: a catalogue of stars with proper motions exceeding 0.5" annually. W J Luyten University of Minnesota, Minneapolis, September ??? ??? 1979 1979 I/98 : NLTT Catalogue (proper motion exceeding 0.2" annually) Proper motions The catalogue gathers stars with large proper motions, the large majority coming out of the Bruce Proper Motion Survey (W.J. Luyten). 804 fields in the Palomar Survey have been hand-blinked or processed by an automated blink-machine; 160 low galactic latitude fields could not be handled. There are therefore many less stars with high proper motion south of -33 degrees (limit of the Palomar Survey) compared to the Northern hemisphere. Stars with proper motions larger than 2arcsec/yr are numbered 1 to 100; stars with proper motions between 1 and 2arcsec/yr are numbered 101 to 1000 ; numbers 1001 through 5000 are assigned to stars with proper motions between 0.5 and 1arcsec/yr. The stars which appear to have motions between 0.480 and 0.499arcsec/yr have been assigned numbers larger than 5000. Numbers larger than 6000 refer to Appendix II of the printed publication, containing stars for which at one time or another a value larger than 0.49arcsec/yr was published; these numbers are not listed in the printed version of the catalogue. All proper motions have been reduced to the Palomar-Bruce system. The catalogue supersedes the "Catalogue of Stars with Motions exceeding 0.5" annually" (LFT) published in 1955 (CDS ref. <I/54>)
The LHS catalogue LHS designation --- Note '*' note detailed in file "notes.dat" --- Name Other designation --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEdm Declination 2000 (deci-minutes) 0.1arcmin RA1950h Right Ascension 1950 (hours) h RA1950m Right Ascension 1950 (minutes) min RA1950s Right Ascension 1950 (seconds) s DE1950- Declination 1950 (sign) --- DE1950d Declination 1950 (degrees) deg DE1950dm Declination 1950 (deci-minutes) 0.1arcmin Rmag Red magnitude mag Pmag Photographic magnitude mag l_Pmag '+' when Pmag is a lower value --- Sp Spectral type --- Color classification based on colour --- pm Total proper motion number=1 the proper motion is empty for LHS 6219, indicated as "plate flaw" in the catalogue. arcsec/yr u_pm Uncertainty flag on proper motion --- pmPA Position angle of proper motion number=1 the proper motion is empty for LHS 6219, indicated as "plate flaw" in the catalogue. deg Disc Original (discovery) name or author --- Notes to LHS stars LHS Star --- Text Text of note --- Francois Ochsenbein CDS 1998 Jul 15 UNKNOWN UNKNOWN * March 1984: first announced in CDS Inf. Bull. 26 * 16-Mar-1995 (version 'A'): reformatted at CDS, transformed to lower-case, and added notes.dat. Duplicate entry LHS 3224 has been deleted Erroneous BD+04 3561 number for Barnard's star (LHS 57) removed * 15-Jul-1998 (version 'B'): following a message by John Gizis (gizis@stratford.phast.umass.edu), two erroneous records (LHS 2297 and 3038) have been corrected. I_87B.xml Accurate Positions of 502 Stars in the Region of the Pleiades 1090 I/90 Positions of 502 Stars in Pleiades Region Accurate Positions of 502 Stars in the Region of the Pleiades H Eichhorn W D Googe C F Lukac J K Murphy MmRAS 73 125 1970 1970MmRAS..73..125E I/163 : U.S. Naval Observatory Pleiades Catalog (Van Flandern 1969) Binnendijk L. 1946, Ann. Sterrew. Leiden, 19, 2 Dieckvoss W. & Kox H. 1955, Astr. Nachr., 282, 217 Eichhorn H. 1960, Astr. Nachr., 285, 233 Eichhorn H. 1970, The Behaviour of Magnitude Dependent Systematic Errors. Paper pres. to Conf. of Phot. Astr. Technique at Tampa FL. Eichhorn H., Googe W. & Gatewood G. 1967, Astr. J., 72, 626 Eichhorn H. & Gatewood G. 1967, Astr. J. 72, 1191 Eichhorn H., Googe W., Lukac C. & Murphy J.K. 1969, USATOPOCOM Tech. Report No. 70 Eichhorn H. & Williams C.A. 1963, Astr. J., 68, 221 Googe W. 1967, Astr. J., 72, 620 Hertzprung E. 1947, Ann. Sterrew. Leiden, 19, 1A Koenig A. 1924, Astron. Nachr., 222, 177 Lacroute P. 1964, Ann. Obs. Strasbourg, 6 Lukac C. 1967, Astr. J., 72, 620 Positional data Proper motions Regional catalog The catalog contains the right ascensions and declinations (equinox B1900.0 and epoch B1955.0) of 502 stars in a region of about 1.5 degrees square in the Pleiades cluster, centered on Eta Tau. These coordinates have been derived from measurements of stellar images obtained with 65 exposures of various durations on 14 photographic plates with two telescopes at McCormick Observatory and Van Vleck Observatory. The plates were reduced by the plate overlap method, which resulted in a high degree of systematic accuracy in the final positions. Data in the machine version include Hertzsprung number, color index, photovisual magnitude, right ascension and declination and their standard errors, proper motion, and differences between the present position and those of Koenig (1924). Data for exposures, plates, and images measured, present in the published catalog, are not included in the machine version.
Data HID Hertzsprung Number 1947 Ann. Sterrew. Leiden, 19, 1A --- B-V Color Index mag mag Photovisual Magnitude mag RAh Right Ascension 1955 hours h RAm Right Ascension 1955 minutes min RAs Right Ascension 1955 seconds s e_RAs Standard Error in Right Ascension s DEd Declination 1955 degrees deg DEm Declination 1955 arcmin arcmin DEs Declination 1955 arcsec arcsec e_DEs Standard Error in Declination arcsec RMSRA RMS for Right Ascension A large RMS indicates that the individual measurements that contribute to a listed coordinate of a certain star show an agreement worse than that expected on the basis of the weighting of the individual measurements; and a small RMS indicates that the positions from the individual measurements of a star agree better than expected. The product 'standard error times RMS' is then a good approximation of the dispersion of the individual contributing positions around their published mean, although not this dispersion itself. --- RMSDE RMS for Declination --- pmRA Proper Motion in Right Ascension Since all positions involved refer to the orientation of the coordinate system at 1900.0, the proper motion components also are valid for 1900.0. Since Konig gives the standard error of his positions as 0.065", and the typical standard error of the reference star's position from this investigation is around 0.03", 0.002" is obtained as the standard error of a proper motion component. This is comparable to, but typically better than the accuracy of Hertzsprung's proper motions. arcsec/ka pmDE Proper Motion in Declination arcsec/ka dpmRA Difference in Proper Motion RA Proper motion in right ascension difference between Hertzsprung's and present work arcsec/ka dpmDE Difference in Proper Motion Dec Proper motion in declination difference between Hertzsprung's and present work arcsec/ka dRA Difference in RA Difference in right ascension between Koenig's and present work positions (1924 Astr. Nachr., 222, 177) carcsec dDE Difference in Dec Difference in declination between Koenig's and present work positions carcsec Julie Anne Watko SSDOO/ADC 1996 Feb 21 I_90.xml Yale Zone Catalogue: Zone -60deg to -70deg 1092 I/92 Yale Zone Catalogue -60 to -70 Yale Zone Catalogue: Zone -60deg to -70deg F W Fallon Yale Trans. 32, part II ??? ??? 1983 1983TOYal..322...1F Astrometric data Proper motions Positional data The original plans for the Southern Yale Zone catalogs were to reobserve and derive strengthened positions and proper motions for all stars in the zones -30 deg to -50 deg and -60 deg to -90 deg. Having been delayed by an incredible number of misfortunes, the zone -60 deg to -70 deg has now been published (Fallon 1983). The catalog contains the measured positions and derived proper motions for the stars in this zone. In addition to the data in the published catalog, this file lists the numbers of the plates measured for each star.
The Catalogue Number Serial number. --- CPD Designation in the Cape Photographic Durchmusterung (CPD, Gill and Kapteyn 1896). --- RAh Right Ascension for Equinox 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination for Equinox 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Epoch Epoch for position. yr pmRAs Annual proper motion in RA s/yr pmRA Annual proper motion in RA (*cos(delta)) arcsec/yr pmDE Annual proper motion in DE arcsec/yr Mag Visual magnitude. mag n_Mag An asterisk indicates constructed magnitude. See note in "adc.doc". Note however that the following stars have very high magnitudes are variables or very late-type stars: Magnitude 19.0 for stars #1707 6181 7370 7883 8852 10606 11237 12261 12614 13157 13236 13868 Magnitude 18.8 for stars #2091 5092 --- CI Color index. mag Images Number of images measured. A pair of grating images is counted as one image. --- Plates Number of plates measured. --- PlateList 18 two-digit numbers identifying plates on which images were measured. If the number measured is less than 18, a zero fill is used for blank fields. --- FieldCode Field star code. This code is always zero, meaning a standard reduction from at least two overlapping plates. See also note in "adc.doc". --- pmCode Proper motion code. See detailed note in "adc.doc". Short explanations: A = Proper motion taken directly from the CPC (therefore on FK3 system). B = Proper motion Yale - LaPlata positions. C = Same as B but mean from overlapping LaPlate positions D = LaPlata position from NFK (Peters 1907) E = Proper motion from Sydney - Yale plates F = Proper motion from mean of Yale/Sydney compared with LaPlata. G = not explained code; exists for stars #13513 13578 13684 13765 13791 #13814 14256 14257 14271 14299 14384 14411 14432 14470 14496 14497 H = not explained code; exists for star #13661 --- adc.doc Document file by Nancy G. Roman and Wayne H. Warren Jr. Francois Ochsenbein CDS 1994 Jul 20 UNKNOWN UNKNOWN Document editing: Nancy G. Roman [SSDOO/ADC] added the key words and description and modified the format table slightly to correspond with the current standard document on 20-Feb-1995. I_92.xml Survey of the Astrographic Catalogue from 1 to 30 degrees of northern declination 1096 I/96 Astrographic Catalogue, +01 to +31 Degrees Survey of the Astrographic Catalogue from 1 to 30 degrees of northern declination A Fresneau Astron. Journ. 88 1378 1983 1983AJ.....88.1378F Astrographic zones Positional data Magnitudes, photographic This machine-readable version of the Astrographic Catalogue (AC), zones +01 to +31 degrees is the result of the determination of mean values for position and magnitude at a mean epoch of observation for each unique star in the original catalogs. The zones considered here (Oxford, Paris, Bordeaux, Toulouse, Algiers [partial]) contained 1,870,976 individual measures, from which the catalog of mean data for 1,025,208 stars was derived. Further analysis by Dr. D.W. Dunham and at the ADC yielded an additional 27897 apparently duplicate entries, which were eliminated to produce the final catalog. The estimated mean standard errors for positional and magnitude data are 0.4 arcsec in each coordinate and 0.4 mag, respectively. Data in this version include <m(pg)>, <Epoch>, <RA> at mean epoch, <DEC> at mean epoch. The mean values are unweighted. No star identifications are provided; hence the user must select stars from the catalog and then identify them in other catalogs or on charts using the equatorial coordinates.
Data RA Right ascension at mean epoch given (1950.0) deg DEC Declination at mean epoch given (1950.0) deg Mphoto Mean photographic magnitude. mag MeanEp Mean epoch of all observations for this star unweighted mean epoch yr M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1996 Mar 08 Appreciation is expressed to A. Fresneau for making the machine-readable catalog available for distribution from the ADC and for reviewing and commenting on a preliminary version of this document. L. H. Wasserman and D. W. Dunham kindly transmitted their findings back to the ADC, and Dr. Dunham supplied his program for elimination of duplicate entries and a copy of his modified version, formatted specifically for ADC purposes. The combined efforts of these colleagues have produced an improved version of the machine catalog for distribution to the astronomical community. The original ADC documentation by Wayne H. Warren, Jr. (1983) was used to create this ReadMe file. Dr. Warren was also responsible for the preparation of the catalog for archiving as described above. UNKNOWN UNKNOWN The machine-readable AC Survey +01 deg to +31 deg was prepared from a tape supplied by the author (A. Fresneau) during a visit to the Astronomical Data Center (ADC) on 21 July 1983. As received, the file was found immediately to contain some stars at various right ascensions which were apparently appended to the file; however, a copy of the unsorted file was supplied to R. L. Millis of Lowell Observatory, where he and L. H. Wasserman found additional groups of stars out of RA order. The arrangement of the data was a result of the reduction procedure (Fresneau 1983c) and should not have been unexpected. Since the stars should be in some kind of rigorous order for data searching purposes, the file was sorted by increasing RA with decreasing DEC as the secondary sort field and increasing magnitude as the tertiary sort field. A copy of the sorted file was then supplied to D. W. Dunham, who discovered 19873 records where all data were identical and 8024 records where differences were too small to be accounted for by duplicity at AC resolution. A separation criterion of 0.00031 deg was used to eliminate all stars whose positions matched to within the limit in both RA and DEC. Since Dunham also changed some of the faint magnitudes to suit his own applications, only his program to eliminate duplicates was used to process the original sorted version to produce the present file with no magnitude modifications and the revised format. Although a more detailed analysis may be performed later, Dr. Warren concurs with the present method and production of this file for distribution until such time as improved criteria may be established. It is important to note and consider the fact that there are quite a few stars present having magnitudes in the 16-18 range and others for which punching errors have occurred, resulting in magnitudes such as 79.3, 79.5, 26.0, 75.3, 49.5, etc. (77 stars fainter than 16 magnitude, including definite punching errors). These errors have not been corrected in the present machine version. I_96.xml Perth 75: a catalogue of positions of 2589 FK4 and FK4S stars 1097 I/97 Perth 75 Catalogue Perth 75: a catalogue of positions of 2589 FK4 and FK4S stars I Nikoloff E Hog Bickley W. Australia, Perth Observatory ??? ??? 1982 1981QB881.N55...... I/62 : The Perth 70 Catalogue of Positions of 24900 Stars (Hog+ 1976) I/143 : FK4 Catalogue (Fricke & Kopff, 1963) I/149 : FK5 Catalogue, part I : Basic Fundamental Stars (Fricke et al. 1988) I/175 : FK5 Catalogue, part II: Extension) (Fricke et al. 1991) Fricke, W., and Kopff, A. 1963, Veroeff. Astron. Rechen-Inst. Heidelb., Nos. 10, 11 (CDS Catalogues <I/143>) Positional data Proper motions Meridian observations Stars, fundamental The catalog contains results of approximately 60000 photoelectric meridian circle observations made at the Perth Observatory for 1156 FK4 and 1433 FK4 Supplement stars south of declination +38 degrees. The catalog reports proper motions and positions at epoch and equinox B1950.0. The data used to derive the epoch 1950 positions are included in the catalog so that originally observed positions may be recomputed and used for geodetic purposes until the FK5 becomes available. The mean error of an individual position in this catalog is 0.07" in right ascension and 0.13" in declination at a zenith distance of 45 degrees, while the mean error of the PERTH 75 system is 0.05" in right ascension and 0.10" in declination. The positions do not contain the large systematic errors of the FK4 (Fricke and Kopff 1963), which can be, for example 0.3" in right ascension for declination < -75 degrees. Data in the catalog included FK4 (FK4S) number, observed visual magnitude, spectral type used for computing refraction, right ascension and declination (equinox and epoch B1950.0), annual proper motion, observed residuals, numbers of accepted observations, and code to indicate if parallax and/or radial velocity has been used in computing apparent positions.
The catalogue Perth 75 FK4 Star number in FK4 (< 2000) or FK4S (> 2000). --- Vmag Observed or FK4 visual magnitude (see n_Vmag) mag n_Vmag An "s" (lower case) if Vmag has been taken from the FK4. --- Sp The HD spectral type --- RAh Right Ascension B1950 (hours) right ascension and declinations at Epoch=B1950.0, referred to equator and Equinox=B1950.0. The determination of the equator and zero point in R.A. was made from observations of approximately 40 FK4 stars per night. h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec pmRA Annual proper motion in R.A. s/yr pmDE Annual proper motion in Dec. arcsec/yr O-C(RA) Observed residual in apparent RA cos(Dec), in the sense Observed minus FK4 or FK4S. 10mas O-C(DE) Observed residual in apparent in Dec., in the sense Observed minus FK4 or FK4S. 10mas o_RAs Number of accepted observations in R.A. --- o_DEs Number of accepted observations in Dec. --- EpRA-1900 Epoch - 1900 for the observation in R.A. yr pFlag A letter "p" (lower case) if parallax and/or radial velocity used in computing apparent positions. --- F. Ochsenbein CDS 1996 Nov 28 This document is just an adaptation of the "Documentation for the machine-readable version of the Perth 75 catalogue" written by Wayne H. Warren Jr. in February 1984. I_97.xml New Luyten Catalogue of stars with proper motions larger than two tenths of an arcsecond (NLTT) 1098A I/98A NLTT Catalogue New Luyten Catalogue of stars with proper motions larger than two tenths of an arcsecond (NLTT) W J Luyten Minneapolis, University of Minnesota ??? ??? 1979 1979 New Luyten Catalogue of stars with proper motions larger than two tenths of an arcsecond (NLTT) W J Luyten H S Hughes Proper Motion Survey with the Forty-Eight inch Schmidt Telescope LV ??? ??? 1980 1980LP.....55....1L Proper motions The NLTT catalog is a collection of stars with proper motions exceeding 0.18"/yr found by Luyten and his coworkers. The First Supplement to the NLTT catalog is the result of continued plate analysis and contains data for 398 stars with proper motions greater than 0.179"/yr. A number of corrections to the data in the published catalog have been entered in the machine-readable version, including the omission of duplicate entries and those stars later determined to show no motion. The catalog contains, in addition to the proper motions, 1950 equatorial coordinates, a flag indicating the approximate accuracy of the positions, estimated red and photographic magnitudes, spectral types, and flags indicating a change from the published volume and the presence of the star in the supplement.
The NLTT Catalogue and 1st Supplement Name Star designation number=1 Identifiers without prefixes are DM (Bonner and Cordoba Durchmusterungen, written with a colon), or Luyten numbers from the Bruce Proper Motion Survey (L numbers) or the Luyten-Palomar Survey (LP numbers), the former in zones -45 to -89 deg and the latter in zones +89 to -44 deg. Other miscellaneous identifiers (Oxf = Oxford AC, Grw = Greenwich AC; U = Upgren; R = Ross, etc...). An asterisk (*) in the identification field indicates that a not exists in the "notes" file of the catalog. --- RAh Hours RA, equinox B1950.0 h RAm Minutes RA, equinox B1950.0 min RAs Seconds RA, equinox B1950.0 s RAm2 Right ascension, equinox B1950.0, minutes only min n_RAs Flag on RA: 1 = RA originally reported in 0.1min --- DE- Sign Dec, equinox B1950.0 --- DEd Degrees Dec, equinox B1950.0 deg DEm Minutes Dec, equinox B1950.0 arcmin Rmag Estimated red magnitude mag n_Rmag Flag on Rmag number=2 ':' indicates a larger uncertainty '+' indicates a mag fainter than reported value 'v' indicates a known variability --- Ptg Estimated photographic magnitude mag n_Ptg '+' Flag on Ptg number=2 ':' indicates a larger uncertainty '+' indicates a mag fainter than reported value 'v' indicates a known variability --- SpType Spectral type; lowercase letters represent estimated color classes or ranges. --- pm Relative proper motion, equinox B1950.0 number=3 The total proper motion is reported. The RA/DE proper motions can be computed with the formulae pmRA = pm.sin(pmPA) pmDE = pm.cos(pmPA) arcsec/yr u_pm ':' if proper motion is uncertain --- pmPA Position angle of PM vector number=3 The total proper motion is reported. The RA/DE proper motions can be computed with the formulae pmRA = pm.sin(pmPA) pmDE = pm.cos(pmPA) deg u_pmPA ':' if position angle is uncertain --- ModFlag 'A' indicates data have been changed (see Appendix A of adc.doc or adc.tex) --- SupplFlag '1' indicates a star from First Supplement (Luyten and Hughes, 1980) --- Remarks for NLTT stars Name Star designation in one of many catalogs --- RAh Hours RA, equinox B1950.0 h RAm Minutes RA, equinox B1950.0 min RAs Seconds RA, equinox B1950.0 s DE- Sign Dec, equinox B1950.0 --- DEd Degrees Dec, equinox B1950.0 deg DEm Minutes Dec, equinox B1950.0 arcmin Text Note for star in free-form text --- adc.doc Documentation by Warren et al. (ascii) doc.tex Documentation by Warren et al. (LaTeX) Francois Ochsenbein CDS 1995 Jun 27 UNKNOWN UNKNOWN * A large number of corrections were performed at ADC, see section 3 of "adc.doc" or "doc.tex" files * From the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory /astrom/nltt * 30-Jun-1995: bad decimal point (blank or dashed) corrected in records 9694 (LP 198-153), column DEm 37692 (LP 381- 80), column pm 38236 (CD-68:1403), column Rmag 52719 (LP 983- 71), column DEm I_98A.xml Meridian Observations made in Brorfelde Copenhagen University Observatory 1964-1967 Photographic 1099 I/99 Brorfelde Meridian Catalogues 1964-1976 Meridian Observations made in Brorfelde Copenhagen University Observatory 1964-1967 Photographic S Laustsen Publ. Mindre Medd. Kbh. Obs. No. 197 ??? ??? 1968 1973A&AS....9....1F Meridian Observations made in Brorfelde Copenhagen University Observatory 1964-1967 Photographic H J Fogh Olsen Astron. Astrophys. Suppl. 9 1 1973 1973A&AS....9....1F Meridian Observations made in Brorfelde Copenhagen University Observatory 1964-1967 Photographic H J Fogh Olsen V Helmer Astron. Astrophys. Suppl. 30 349 1977 1977A&AS...30..349O Meridian Observations made in Brorfelde Copenhagen University Observatory 1964-1967 Photographic V Helmer H J Fogh Olsen Astron. Astrophys. Suppl. 49 13 1982 1982A&AS...49...13H Meridian Observations made in Brorfelde Copenhagen University Observatory 1964-1967 Photographic L Helmer C Fabricius O H Einicke C Thoburn Astron. Astrophys. Suppl. 53 223 1983 1983A&AS...53..223H Meridian Observations made in Brorfelde Copenhagen University Observatory 1964-1967 Photographic L Helmer C Fabricius O H Einicke C Thoburn L V Morrison Astron. Astrophys. Suppl. 55 87 1984 1984A&AS...55...87H Positional data Meridian observations This catalog contains positions and magnitudes for 1577 stars with visual magnitudes brighter than 11.0. The observations were made with the 7-inch transit circle at the Copenhagen University Observatory from July 1981 to May 1982. The positions are reduced to the FK4 system for each night and over the whole meridian. The mean errors of the catalog entries are: in right ascension 0.006 seconds/cos(declination); in declination, 0.10"; and in magnitude, 0.06mag. The catalog contains 425 FK4 stars used for the adjustment to the FK4; 167 stars from the AGK3 zones +88deg. and +89deg.; 115 stars from the zone around the North Galactic Pole; stars from several PZT zones; some faint GC stars; reference stars for radio fields; and a few stars from earlier Brorfelde programs. The internal errors of a single observation are for right ascension, 0.0138 seconds/cos(delta), for declination, 0.216", and for the magnitude, 0.132 mag.
Brorfelde Photographic Meridian Catalogues ID Internal number --- BDsign BD zone sign --- BDzone BD zone --- BDnum BD number within zone --- BDsuf BD suffix --- AGK3sign AGK3 zone sign --- AGK3zone AGK3 zone --- AGK3num AGK3 number within zone --- AGK3suf AGK3 suffix --- FK4 FK4 or NPZT number For FK4 no other reference is given. --- GC GC number --- mag Approximate visual magnitude 10-2mag Sp Spectral Type --- RAh Right Ascension (1950.0) hours h RAm Right Ascension (1950.0) minutes min RAs Right Ascension (1950.0) seconds s o_RAs Number of observations in Right Ascension --- EpRA Epoch - 1900 for RA a plxRA Parallax factor in RA * 100 --- DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin DEs Declination (1950.0) arcseconds arcsec o_DEs Number of observations in Declination --- EpDE Epoch - 1900 for Dec a plxDE Parallax factor in Dec * 100 --- ADS ADS or BDS number 0 = neither ADS nor BDS number given AY = ABC AX = A' --- Brorfelde Photoelectric Meridian Catalogues cat Catalogue identification 001 = Helmer et al. =1983A&AS...53..223H 002 = Helmer at al. =1994A&AS...55...87H program stars 003 = Ibid. FK4 stars (no cross references are given) --- ID1 Identification number within catalogue --- ID2 Internal identification --- RAh Right Ascension (1950.0) hours h RAm Right Ascension (1950.0) minutes min RAs Right Ascension (1950.0) seconds s o_RAs Number of observations in RA --- EpRA Epoch of observation for RA a DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin DEs Declination (1950.0) arcseconds arcsec o_DEs Number of observations in Dec --- EpDE Epoch of observations in Dec a mag Observed magnitude mag o_mag Number of observations in mag --- Sp Spectral type --- DMsign Durchmusterung zone sign --- DMzone Durchmusterung zone --- DMnum Durchmusterung number within zone --- DMsuf Durchmusterung suffix --- AGK3sign AGK3 zone sign --- AGK3zone AGK3 zone --- AGK3num AGK3 number within zone --- SAOC SAOC number --- HD HD number --- GC GC number --- FK4 FK4 or FK4 Sup number --- n_FK4 * = program star --- Gleise Gleise number --- ADS ADS number --- ADSsuf ADS suffix --- ignore Asterisk --- Julie Anne Watko SSDOO/ADC 1996 May 07 I_99.xml Cape Photographic Durchmusterung (CPD) Part I: zones -18 to -37 degrees 1108 I/108 Cape Photographic Durchmusterung Cape Photographic Durchmusterung (CPD) Part I: zones -18 to -37 degrees D Gill J C Kapteyn Cape Photographic Durchmusterung, Ann. Cape Obs. 3 ??? ??? 1895 1896AnCap...3....1G Cape Photographic Durchmusterung (CPD) Part I: zones -18 to -37 degrees D Gill J C Kapteyn Cape Photographic Durchmusterung, Ann. Cape Obs. 4 ??? ??? 1897 1897AnCap...4....1G Cape Photographic Durchmusterung (CPD) Part I: zones -18 to -37 degrees D Gill J C Kapteyn Cape Photographic Durchmusterung, Ann. Cape Obs. 5 ??? ??? 1900 1900AnCap...5....1G Surveys Durchmusterungen The "Cape Photographic Durchmusterung" (CPD, Gill and Kapteyn 1895-1900) is a photographic survey of southern stars in the declination range -18 deg to -90 degrees. The original goal of the work was to carry out a southern survey similar to those of the "Bonner Durchmusterung" (BD, Argelander 1859-1862, see also Kuestner 1903) and Schoenfeld (1886) and the "Cordoba Durchmusterung" (CD, Thome 1892-1932) but using photographic plates which would provide a permanent record of the sky at the epoch of observation. The summary of the positional uncertainties quoted in the third volume of the published catalog gives +/- 0.28 sec (R.A.), +/- 0.044 arcmin (Dec.) for zones -18 to -57 degrees, +/- 0.157 sec + 0.0764/cos(delta) sec (R.A.), +/- 0.056 arcmin (Dec.) for zones -58 to -85 degrees, and +/- 0.157 sec + 0.0353/cos(delta) sec (R.A.), +/- 0.0127 arcmin (Dec.) for the polar plate where, as explained in the intro- duction to the third volume, many positions were derived from rectangular coordinates (these are positions reported to 0.1 sec (R.A.) and 0.001 arcmin (Dec.) in the -86 to -89 degree zones in the catalog). The probable error of a photographic magnitude, as determined by combining results for different magnitudes and weighting proportionately according to the numbers of stars in each class of magnitude, is given as +/- 0.055 mag. From an analysis of the faint magnitude limits on the plates discussed in the third volume introduction, the catalog as a whole can be considered complete to photographic magnitude 9.2, but it is stated that it will be found practically complete, in or near the Milky Way, to magnitude 9.5.
The complete catalog is contained in the data file, and corrections published in all errata have been made to the data. The machine version contains 454877 records, but only 454875 stars (two stars were later deleted, but their logical records are retained in the file so that the zone counts are not different from the published catalog). A list of corrections made to the original data as a result of errata published in the three volumes is presented in cpchg.dat. No other corrections or changes have been incorporated into the original data, e.g., from more modern positions and magnitudes or comparison with other catalogs. The original ADC document contains the total number of stars in each declination zone and the number added and deleted in each zone. Data are present for all stars in the catalog, including some which have been deleted in the errata; these have been flagged by a "D" in byte 11 of each respective record, but the records and data have been left in the machine version in order not to change the star counts and numerical sequencing and so that the stars appear in the correct locations if the catalog is sorted by right ascension.
The CPD catalog cat The catalog prefix --- zonesign The sign of the declination zone --- zone The declination zone deg num The number of the star within the zone --- suppl star in corrigenda a, b, or c: star is added in the corrigenda; D: star is deleted in the corrigenda --- mag Estimated photographic magnitude 20.0 = neb; 30.0 = var mag RAh Hours of right ascension, 1875 h RAm Minutes of right ascension, 1875 min RAs Seconds of right ascension, 1875 precision varies; tenths can be blank s DE- Sign of declination --- DEd Degree of declination, 1875 deg DEm Minutes of declination, 1875 Only bytes 27-30 are used in zones north of -86 deg; the complete field is used for many stars on the polar plate. arcmin Changes from the printed cat. zonesign The sign of the CP zone --- zone The CP zone --- num The CP number --- n_num Note on star number --- field The field changed --- old The printed value --- new The corrected value --- note Comments --- adc.doc The original ADC document Nancy G. Roman NSSDC/ADC 1994 Nov 12 This project owes its completion to the extensive work and striving for perfection of Barry Rappaport, who supervised the punching of all data, ran numerous machine and manual checks on completed zones, and prepared the preliminary tape of the finished catalog. The quality work of the keypunchers at Case Western Reserve University and Syntronix, Sherman Oaks, California is also greatly appreciated. The encouragement and support of the NSSDC Director, James I. Vette, made the completion of this project possible. This document is based on the original ADC document prepared by Wayne H. Warren, Jr. UNKNOWN UNKNOWN The data in the machine-readable "Cape Photographic Durchmusterung" were keypunched directly from the published catalogs. The northern zones (-18 to -32 degrees and -35 degrees) were punched at Case Western Reserve University under the direction of B. N. Rappaport, who initiated the work and used the data as part of a project on the production of star charts by computer. However, only zones -18 through -26 degrees and -28 degrees had been verified and checked thoroughly, and some zones had not been completed. Mr. Rappaport was contacted and volunteered to continue the project and to oversee the punching and verifying of the remaining zones and those not verified and checked at Case. These zones were processed by a commercial firm with funding provided by the National Space Science Data Center, but all systematic checking of the completed zones was carried out by Mr. Rappaport on a volunteer basis. The zones were rechecked for counts and errata corrections, and the data reformatted to the standard DM catalog structure at the ADC by the author. The individual zones were then concatenated from disk data sets to a single magnetic tape file in CPD number order from north to south. Users should note that, due to corrections inserted from the errata, the CPD stars are not strictly in right ascension order within each zone; hence, if the catalog is sorted by right ascension, e.g., for search purposes, some CPD numbers will become disordered. I_108.xml Catalogue of Occultation Double-Star Observations 1110 I/110 Occultation Double-Star Observations Catalogue of Occultation Double-Star Observations D S Evans IAU Colloquium No. 62, Current Techniques in Double and Multiple Star Research, Lowell Obs. Bull. 167, p. 73 ??? ??? 1983 1983LowOB.167...73E Stars, double and multiple Occultations This catalog contains data on 224 double stars observed photoelectrically during lunar occultations. The author cites the advantages of this method of double star detection as increased resolution, accuracy of the vector separations of roughly one-half arcsecond or better, and the opportunity to make photometric determinations of the magnitude differences between components. The vector separation is the true separation projected along a line perpendicular to the actual lunar limb. The catalog is a compilation of twelve years of observations from the literature (through roughly 1980). It is divided into three files. The first file, data1.dat, contains information on stars brighter than visual magnitude 6.7. The second, data2.dat, lists SAO catalog stars fainter than magnitude 6.7. The third file, data3.dat, contains data on faint stars with no SAO number. For these stars, data on their magnitudes or spectral types may be absent. In many cases there are multiple records per star, reflecting separate observations. The records are arranged by SAO number or other identifier, and contain visual magnitudes, spectral type, observing run number, a subjective grade of the probability of being double, the vector separation with computed error, position angle, and the lunar limb slope and its error. It also includes the magnitude difference between the components in (somewhat arbitrarily assigned) blue and red band passes. In the case of a triple star, the run number is repeated and the data for the triple given with magnitude differences from the brightest star.
m(v) <= 6.7 SAO SAO Number --- NAME Other Name for Star --- MAG Magnitude mag Sp Spectral Type --- RUN Run Number of the Observation Sources McDonald Observations: M100-1871: Astron. J. 76, 1109, 1971: M1875-M1893, M2102-M22221, M2304-2711: Astron. J. 78, 482, 1973: M1902-M2020, M2250-2262: Astron. J. 80, 449, 1975: M2713-M3712: Astron. J. 80, 689, 1975: M3713-M4009: Astron. J. 81, 650, 1976: M4010-M4245, Astron. J. 82, 631, 1977 (but M4045, M4058, M4059, M4148, Astron. J. 82, 640, 1977): M36/7, M36/8, M4247-M4729: Astron. J. 83, 1100, 1978: M4730-M5222, Astron. J. 85, 478, 1980 (but M5100-M5112: Astron. J. 85, 490, 1980), and M5223-M5646, Astron. J., submitted. Geneva Observations: G12-G38: Astron. J. 80, 445, 1975. Tonantzintla Observations: T001-023: Astron. J. 79, 1299, 1974. Iowa Observations: EB002, EB021: Astron. J. 76, 1131, 1971: EB001-EB121, Astrophys. J. Supp. Ser. 28, 405, 1974: EB122-EB320, : Astrophys. J. Supp. Ser., 34, 493, 1977: EB321-562: Astrophys. J. Supp. Ser., 40, 475, 1979: EB585-592: Astrophys. J. Lett. 228, Llll, 1979. Hamburg Observations: All H numbers, Astron. Astrophys., 48, 245, 1976. Victoria Observations: Vl-V2: Publ. Dom. Astrophys. Obs. 14, 271, 1974: Vl-V32, J. Roy. Astron. Soc. Canada, 72, 305, 1978. Illinois Observations:-I7701-I7865: Astron. J. 85, 1053, 1980. Flagstaff Observations: F, Astron. J. 84, 872, 1979 and private communications. Peterson et al.: P: Astron. J. 86, 280, 1981. Special Stars: Beta Scorpii: Astron. J. 82, 414, 1977. Astron. J. 82, 495, 1977, Astron. J. 83, 438, 1978: Astron. J. 84, 257, 1979. Sigma Scorpii: Publ. Astron. Soc. Pac. 86, 116, 1974. Beta Capricorni: Astrophys. J. 228, 497, 1979. --- DAY Observation Date Day --- MONTH Observation Date Month --- YEAR Observation Date Year --- G Grade 0 No Duplicity 1 Possible Duplicity 2 Probable Duplicity 3 Certain Duplicity Grades are based on statements by observers. --- n_G Remark on G Asterisks (*) denote places where corrections have been applied to published figures, whether errors of star numbers or run numbers in original records or notes. Most commonly corrections have been made as far as can be deduced from the original sources, to bring the column of position angle values to those appropriate to position angles from the brighter to the fainter component. Most changes have been made by 180 degrees. --- SEP Vector Separation marcsec e_SEP Computed Error of Vector Separation marcsec n_SEP Remark on SEP (see note on n_G) --- PA Position Angle Position Angle on the lunar limb as modified by the slope deduced in favorable cases from the spacing of the diffraction bands on the occultation trace. deg n_PA Remark on PA (see note on n_G) --- SL Limb Slope --- n_SL Remark on SL (see note on n_G) --- e_SL Error of SL --- dB Blue Differential Magnitude mag e_dB Error of dB mag n_dB Remark on dB An asterisk indicates that the magnitude difference between components had to be computed from values expressed in different style in the original papers. --- dR Red Differential Magnitude A negative sign indicates that the "secondary" is fainter in the blue channel and brighter in the red. mag e_dR Error of dR mag n_dR Remark on dR (see note on n_dB) --- SAO m(v) > 6.7 SAO SAO Number --- SAOsuf SAO Suffix --- NAME Other Name for Star --- MAG Magnitude mag Sp Spectral Type --- RUN Run Number of the Observation see note for data1.dat --- DAY Observation Date Day --- MONTH Observation Date Month --- YEAR Observation Date Year --- G Grade see notes for data1.dat --- n_G Remark on G see notes for data1.dat --- SEP Vector Separation marcsec e_SEP Computed Error of Vector Separation marcsec n_SEP Remark on SEP (see note on n_G) --- PA Position Angle see notes for data1.dat deg n_PA Remark on PA (see note on n_G) --- SL Limb Slope --- n_SL Remark on SL (see note on n_G) --- e_SL Error of SL --- dB Blue Differential Magnitude mag e_dB Error of dB mag n_dB Remark on dB see notes for data1.dat --- dR Red Differential Magnitude see notes for data1.dat mag e_dR Error of dR mag n_dR Remark on dR (see note on n_dB) --- Faint Non-SAO DM DM Number --- NAME Other Name for Star --- MAG Magnitude mag Sp Spectral Type --- RUN Run Number of the Observation see notes for data1.dat --- DAY Observation Date Day --- MONTH Observation Date Month --- YEAR Observation Date Year --- G Grade see notes for data1.dat --- n_G Remark on G see notes for data1.dat --- SEP Vector Separation marcsec e_SEP Computed Error of Vector Separation marcsec n_SEP Remark on SEP (see note on n_G) --- PA Position Angle see notes for data1.dat deg n_PA Remark on PA (see note on n_G) --- SL Limb Slope --- n_SL Remark on SL (see note on n_G) --- e_SL Error of SL --- dB Blue Differential Magnitude mag e_dB Error of dB mag n_dB Remark on dB see notes for data1.dat --- dR Red Differential Magnitude see notes for data1.dat mag e_dR Error of dR mag n_dR Remark on dR (see note on n_dB) --- Julie Anne Watko SSDOO/ADC 1995 Nov 03 I_110.xml Lowell Proper Motion Survey - Southern Hemisphere Catalog 1978 1112 I/112 Lowell Proper Motion Survey - Southern Hemisphere Lowell Proper Motion Survey - Southern Hemisphere Catalog 1978 H L Giclas R Burnham Jr. N G Thomas Lowell Observatory Bulletin No. 164, ??? ??? 1978 1978LowOB...8...89G I/79 : Lowell Proper Motion Survey in Northernern Hemisphere (Giclas+ 1971) Giclas H.L., Burnham JR. R., and Thomas N. G. 1971, Lowell Proper Motion Survey, Northern Hemisphere, The G Numbered Stars (Flagstaff: Lowell Observatory). Giclas H.L., Burnham Jr. R., and Thomas N. G. 1978, Lowell Proper Motion Survey, Southern Hemisphere Catalog 1978, Lick Obs. Bull. No. 164. Positional data Proper motions This catalog contains a summary of the Lowell Proper Motion Survey for the southern hemisphere as completed to mid-1978. The catalog gives the position, motion, magnitude, and color of 2758 stars from the Lowell program.
The material from which this catalog has been prepared is drawn from Lowell Observatory Bulletins, in which the data have been published from 1958 to 1978. The number of the specific Lowell Bulletin where the object was first identified and measured and a finding chart given is given in the eighth column of the catalog under the heading CHT. The first epoch plates were taken in connection with the trans-Neptunian planet search beginning late in the year 1929. The second epoch matching plates were taken as the blinking and measuring progressed, Therefore the difference in epoch increased from a minimum of 28 years at the beginning of the survey to 48 years as of the date of this catalog. At the inception of the program, a reasonable degree of completeness could be maintained for motions of 0.27"/year and larger. Later in the program the limit was lowered to include motions of 0.20"/year and larger. This catalog, therefore, is a combination of these two limits of motions; however, the percentage of plate regions with the smaller motion limit is much greater in this southern hemisphere catalog than in the northern hemisphere. The four plate regions around the south galactic pole are all measured to the lower limit of motion.
The catalog G Original G number assigned Byte 1 of the field always contains a G and byte 5 always contains a -. The number in bytes 2-4 is the plate number, while that in bytes 6-8 is the star number on the plate. Original G number assigned to the star on the plate region where it was first found. Stars that were subsequently found on later plates were assigned new G numbers; however, in this catalog all duplicate observations have been combined and averaged with the original G numbers retained. In cases where a close companion has been found on a later plate, the source of a finding chart prepared from that plate may be found in the identification chart field (ref2). When the catalog entry is a mean formed from two or more observations, the additional stars making up the mean are listed first in the References field (ref). --- flag Note in the printed catalog An asterisk (*) indicates that a note concerning the star appears in the Bulletin in which it was first published. The reference to the original report of the motion is as follows: ---------------------------------------------------- Volume Page No. Year G Region ---------------------------------------------------- IV 136 102 1959 G1 -G50 V 61 112 1961 G51 -G100 VI 1 120 1964 G101-G150 VI 103 122 1964 G151-G160 VI 135 124 1964 G161-G170 VII 217 158 1972 G266-G269 VII 273 160 1973 G270-G271 VIII 9 162 1975 G272-G273 VIII 59 163 1978 G274-G275 --- RAh Right ascension hours (Equinox 1950) h RAm Right ascension minutes min RAs Right ascension seconds s DE- Declination sign (Equinox 1950) --- DEd Declination degrees deg DEm Declination arcminutes arcmin pm Annual total proper motion The annual proper motion in seconds of arc. The proper-motion vector is defined by the equation: pm = (mu(alpha)**2*cos(delta)**2+mu(delta)**2)**0.5 arcsec/yr pmPA Proper motion position angle The position angle of the reported motion in the usual notation from the north point through east, 0deg. to 360deg.. The position angle of pm is defined by the following set of equations: mu(alpha)*cos(delta) = pm*sin(pmPA); mu(delta) = mu*cos(pmPA) deg Pmag Estimated Photographic (blue) magnitude mag col Color class The estimated color class is on a scale from -2 (the bluest) to +4 (the very reddest) stars found. Almost all stars of color classes -2 and -1 have been subsequently identified from photometry or spectra as white dwarfs. Because there is such a wide variety of different types of objects among these motions, it is impossible to define a narrow relationship between these color classes and the conventional B-V and U-B colors. The table below is given with the warning that the true color of any one individual star may deviate from the mean value by as much as half a magnitude for stars redder than color class 0. --------------------------------- Color Class B-V U-B --------------------------------- -1 +0.11 -0.74 0 +0.26 -0.57 +1 +0.80 +0.33 +2 +1.30 +1.09 +3 +1.61 +1.18 --- X-id Other identifications Catalog entries are, in many cases, the combined means of measurements on two or more plate regions; in these cases, the additional G number(s) appear as the first entry(ies) in the Reference field. If a G number in the references carries an asterisk, but the field following the identification field (byte 9) does not, then the note on that star appears only in the Lowell Observatory Bulletin where the latter number was published. Following the G numbers, references to other proper-motion lists and catalogs are given, as identified in the reference key in the appendix of this document. --- LOBchart Identification chart reference The Lowell Bulletin number in which an identification chart of size 18 minutes of arc on a side is given for the star. The summary catalog was compiled from collections of data appearing in earlier Lowell Observatory Bulletins. There are no finding charts in the source reference, but they can be found in the original references given in the table of the Note on n_ID. --- References of used acronyms Acronym Designation of catalog or list The references to other proper-motion catalogs and lists are identified by character prefixes, followed by the numerical designations of the objects in a catalog or list, according to standard astronomical usage. The prefixes are identified with their corresponding references. (Note: Not all of the identifiers listed actually appear in the catalog. The key is repeated from the Lowell Proper Motion Survey, Northern Hemisphere (Giclas, Burnham, and Thomas 1971) and some identifiers may only appear in that catalog.) Reference Sources (= in column Sep) The bibliographical sources that provided information for the catalog consist of references for the star designations in other catalogs and lists, plus references for general information. The general references are combined with some supplementary identification references in the source publications and that order has not been changed in the following sections. The information given below appears in the source reference and is repeated here for users who do not have ready access to that publication. Supplementary References (: in column Sep) The supplementary references include sources of some identifiers used in the catalog, plus general reference sources consulted during preparation of the catalog. --- Sep original list (=) or supplement (:) --- Text Text of Reference --- Julie Anne Watko SSDOO/ADC 1995 Dec 08 A tape copy of the G-numbered stars was kindly supplied by H.L. Giclas to CDS in January 1985. I_112.xml General Catalogue of 33342 stars (Version 1985) 1113A I/113A General Catalogue of 33342 stars General Catalogue of 33342 stars (Version 1985) B Boss Carnegie Inst. of Wash. Publ. 468 ??? ??? 1937 1937gcse.bookQ....B Fundamental catalog Positional data Proper motions Stars, fundamental The GC is a catalog of standard positions and proper motions for (all) stars brighter than magnitude 7, extending from the north to south celestial poles. Several thousand additional stars promising to yield reasonably accurate proper motions were included in the catalog. The objectives of the work were to provide standard positions and motions of accuracy limited only by the character and abundance of the observational material upon which the data were based and thus to provide a rich supply of data to promote research in many astronomical fields. The machine version of the GC includes both The Henry Draper Catalogue and Durchmusterung identifications for all stars, although the published GC contains only one or the other. The 1985 version corrected many errors present in a previous machine version and included probable errors for the positions and centennial proper motions (not present in the previous version). In this version decimal points have been aligned for all but a very few of the secular variations and third terms. These quantities are given with the same precision as in the printed catalog, and the coded spectral types have been omitted. The following quantities are included in the machine but not the published version: galactic coordinates and DM numbers. The following data are in the published but not the machine version: centennial increments of proper motion in right ascension and declination, probable errors of the right ascension and declination at 1950.0, and remarks. The documentation supplied with the machine catalog gives a byte-by-byte format description, indigenous catalog characteristics, code explanation tables, and changes incorporated to produce this and previous Astronomical Data Center versions.
The General Catalogue GC Boss General Catalog (GC) number --- Vmag Visual magnitude, '9999' indicates variability number=1 All magnitudes are given to two decimal places in the computer-readable version. Magnitudes underlined in the published version of the catalog are not indicated on the computer-readable version. 0.01mag SpType Spectral type --- RAh Hours RA, equinox 1950.0, epoch 1950.0 h RAm Minutes RA, equinox 1950.0, epoch 1950.0 min RAs Seconds RA, equinox 1950.0, epoch 1950.0 s EpRA Mean epoch of RA observations number=4 The first two digits of the year are omitted. Thus 98.8 should be read 1898.8 and 05.3 should be read 1905.3. a AvarRA Annual variation of precession in RA number=3 The number of decimals can be smaller for positions close to one of the poles (see document) s/a SvarRA Secular variation in precession in RA number=3 The number of decimals can be smaller for positions close to one of the poles (see document) 0.1ms/a2 Term3RA Third term in precession in RA number=3 The number of decimals can be smaller for positions close to one of the poles (see document) us/a3 pmRA Proper motion in RA s/a DE- Sign Dec, equinox 1950.0 --- DEd Degrees Dec, equinox 1950.0, epoch 1950.0 deg DEm Minutes Dec, equinox 1950.0, epoch 1950.0 arcmin DEs Seconds Dec, equinox 1950.0, epoch 1950.0 arcsec EpDE Mean epoch of DE observations number=4 The first two digits of the year are omitted. Thus 98.8 should be read 1898.8 and 05.3 should be read 1905.3. a AvarDE Annual variation of precession in DE number=3 The number of decimals can be smaller for positions close to one of the poles (see document) arcsec/a SvarDE Secular variation in precession in DE number=3 The number of decimals can be smaller for positions close to one of the poles (see document) 0.1mas/a2 Term3DE Third term in precession in DE number=3 The number of decimals can be smaller for positions close to one of the poles (see document) uarcsec/a3 pmDE Proper motion in Dec arcsec/a Remark Coded remarks number=2 Remarks are defined as follows: 0 = No remark given 1 = Spectrum given 2 = Aitken or Innes number given 3 = Aitken or Innes number given with each component having a separate GC number 4 = Other information given 5 = 1+2 6 = 1+3 7 = 1+4 8 = 2+4 9 = 3+4 - = 1+2+4 + = 1+3+4 --- DM Durchmusterung designation: catalog in bytes 101-102: 'BD', 'CD', 'CP' catalog number in bytes 103-110: SZZNNNNN component identification in bytes 111-112 BD supplement letter in byte 113 --- GLON Galactic longitude deg GLAT Galactic latitude deg HD Henry Draper Catalog (HD) number --- m_HD HD component/multiple code number=5 The HD component code takes the following values: 0 for single stars or brighter components of doubles with difference in visual magnitude > 0.3mag. 1 designates the brighter component, not necessarily A, for doubles with difference in visual magnitude <= 0.3mag 2 designates the fainter component, not necessarily B, for doubles with difference in visual magnitude <= 0.3mag 9 indicates that two successive HD numbers (HD and HD+1) refer to the same SAO star. --- e_RA Probable error in RA at epoch arcsec e_pmRA Probable error in RA proper motion 10mas/a e_DE Probable error in DE at epoch arcsec e_pmDE Probable error in DE proper motion 10mas/a Modifications History GC Boss General Catalog (GC) number --- Field Field Changed --- Printed Old Value --- New Current Value --- adc.doc Documentation in plain ascii by ADC doc.tex ADC document in LaTeX Francois Ochsenbein CDS 1995 Oct 13 UNKNOWN UNKNOWN * See section 4 "Remarks and Modifications" in the document file (adc.doc or doc.tex), and the list of modifications in file "changes.dat" * A previous version is on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (October 1991), directory /astrom/gc * This standardized "ReadMe" document file was written in October 1995 at CDS (Francois Ochsenbein), using the ADC documentation written by Nancy G. Roman and Wayne H. Warren Jr. I_113A.xml Cordoba Durchmusterung 1114 I/114 Cordoba Durchmusterung Cordoba Durchmusterung J M Thome Resultados del Observatorio Nacional Argentino 16 Part I: -22deg to -32deg ??? ??? 1892 1892cdbp.book.....T Cordoba Durchmusterung J M Thome Resultados del Observatorio Nacional Argentino 17 Part II: -32deg to -42deg ??? ??? 1894 1894cdbp.book.....T Cordoba Durchmusterung J M Thome Resultados del Observatorio Nacional Argentino 18 Part III: -42deg to -52deg ??? ??? 1900 1900cdbp.book.....T Cordoba Durchmusterung J M Thome Resultados del Observatorio Nacional Argentino 21 Part I: -52deg to -42deg) ??? ??? 1914 1914cdbp.book.....T Cordoba Durchmusterung J M Thome Resultados del Observatorio Nacional Argentino 21 Part IV: -52deg to -42deg) ??? ??? 1914 1914cdbp.book.....T Cordoba Durchmusterung J M Thome Resultados del Observatorio Nacional Argentino 21 Part II: -62 deg to -90deg) ??? ??? 1932 1932cdbp.book.....T Cordoba Durchmusterung J M Thome Resultados del Observatorio Nacional Argentino 21 Part V: -62 deg to -90deg) ??? ??? 1932 1932cdbp.book.....T Surveys Durchmusterungen The "Cordoba Durchmusterung" (CD, Thome 1892-1932) is a visual survey of southern stars in the declination zones -22 to -89 deg, carried out as an extension to the "Bonner Durchmusterung" (BD) catalogs of Argelander (1859-1862) (see also Kuestner 1903) and Schoenfeld (1886). It contains 613959 records for stars brighter than 10.0 magnitude.
The goal of the survey was to obtain a position and estimated visual magnitude for every star down to 10.0 magnitude inclusive, but the faint limit was confirmed from comparisons with other catalogs, to be somewhat below 10. The positional uncertainties quoted in the original publications vary from +/- 0.42 sec and +/- 0.23 arcmin for zones -22 to -32 deg and +/- 0.33 sec, +/- 0.10 arcmin for zones -42 to -51 deg. The document originally prepared by Wayne H. Warren Jr., on which this document is closely based (adc.doc) contains substantial additional information.
The CD catalog cat The catalog prefix --- zonesign The sign of the declination zone --- zone The declination zone deg num The number of the star within the zone --- suppl star in corrigenda a, b, or c: star is added in the corrigenda; D: star is deleted in the corrigenda --- mag Estimated visual magnitude 20.0 = neb; 30.0 = var mag RAh Hours of right ascension, 1875 h RAm Minutes of right ascension, 1875 min RAs Seconds of right ascension, 1875 precision varies; tenths can be blank s DE- Sign of declination --- DEd Degree of declination, 1875 deg DEm Minutes of declination, 1875 arcmin Changes from the printed cat. zonesign The sign of the CP zone --- zone The CP zone --- num The CP number --- n_num Note on star number --- field The field changed --- old The printed value --- new The corrected value --- note Comments --- adc.doc The original ADC document Nancy G. Roman NSSDC/ADC 1994 Nov 12 Although the work was initiated and supervised by Jaylee M. Mead, Theresa A. Nagy and Wayne H. Warren Jr., punching could never have been begun and the project completed without the support and encouragement of the NSSDC Director James I. Vette. The keypunching was done at NSSDC by Beth Alexander, Carol Bergstrom and Margy Goodwin, while the monitoring software for the data transfer was written by Frank Barnes with contributions by Eugene Scarzafava, and data migration to tape was done by Charleen Perry with assistance and supervision by Ralph Post. Proofreading of individual zones was contributed by Scott Birney (Wellesley College), Richard Dietz (University of Northern Colorado), Mati Morel (Rankin Park, NSW, Australia), Theresa Nagy (ADC), Sidney Parsons (Space Telescope Science Institute), William Stein (U. S. Naval Surface Weapons Laboratory, Dahlgren, VA), George Wolf (Southwest Missouri State University), and the author. Additional zones were proofread at the ADC by summer students Paula Feldman and Kimberly Kniffen, who also assisted greatly with error checking, recording, and data correction. Checking and recording were also done at the ADC by Rajendra Nigam, Charleen Perry and the author. UNKNOWN UNKNOWN The data in the machine-readable "Cordoba Durchmusterung" were keypunched directly from the published catalog at the National Space Science Data Center (NSSDC). The original catalog had been microfiched earlier by photocopying and filming the entire printed version, and copies of the microfiche had been distributed to interested members of the astronomical community. Ten volunteers from the U.S. and Australia completed the proofing over the next three years. Individual zones from the complete preliminary tape were then transferred to disk storage and edited. This method was used to provide further checks where errors might be recognized during the correction process. as that zone was being processed. After the correction of all zones, the individual data sets were concatenated to a single magnetic tape file. This Users should particularly note that, due to corrections inserted from the corrigenda, the CD stars are not strictly in right ascension order within each zone; hence, if the catalog is sorted by R.A., e.g., for search purposes, some CD numbers will become disordered. On the other hand, if right ascension searching is to be performed, it will be necessary to sort the catalog by right ascension. All corrections made to the original catalog by incorporation of the corrigenda are presented in cdchg.dat where it is noted when stars have become disordered in right ascension following the changes. I_114.xml Cape Photographic Catalogue for 1950.0 zone -30 to -64 1116 I/116 Cape Photographic Cat. 1950.0 Cape Photographic Catalogue for 1950.0 zone -30 to -64 J Jackson R H Stoy Ann. Cape Obs. 17 ??? ??? 1954 1954AnCap..17...40J Cape Photographic Catalogue for 1950.0 zone -30 to -64 J Jackson R H Stoy Ann. Cape Obs. 18 ??? ??? 1955 1955AnCap..18.....J Cape Photographic Catalogue for 1950.0 zone -30 to -64 J Jackson R H Stoy Ann. Cape Obs. 19 ??? ??? 1955 1955AnCap..19.....J Cape Photographic Catalogue for 1950.0 zone -30 to -64 J Jackson R H Stoy Ann. Cape Obs. 20 ??? ??? 1958 1958AnCap..20.....J Cape Photographic Catalogue for 1950.0 zone -30 to -64 R H Stoy Ann. Cape Obs. ??? ??? 1966 1966AnCap..21.....S Positional data Proper motions Magnitudes, photographic Photographic catalog This catalog includes most of the stars from the 1900.0 Cordoba Zone Catalogues B and C in the zone -30 deg. -35 deg. at the equinox of 1925.0. Some of the fainter Cordoba stars have been omitted in the rather crowded regions in the Milky Way. The aim was to provide accurate places for an average of 9 to 10 stars per square degree as a reference for a rereduction of the AG positions. Most of the stars have visual magnitudes between 7 and 10. Positions and proper motions have been supplied from the General Catalogue for those stars that were too bright for accurate measurement on photographic plates. The positions are on the FK3 system for the equinox of 1950.0. The probable errors of the positions are nominally +/- 0.15" in both right ascension and declination. That of the proper motions should not exceed +/- 1.4"/century, or +/-14 in the units in which the proper motions expressed in arc are given in the catalog.
Whenever possible, proper motions are derived by comparison with earlier visual observations but for many of the stars in the more southerly zones, no earlier observations exist. The magnitudes were determined from a series of in-focus photographs in both photographic and visual sensitivities. They are on the system defined by "Standard Magnitudes in the E Regions" (Cape Mimeogram No. 3, 1953). Although the resulting magnitudes are fairly close to this system, a small change of color equation with magnitude has not been completely eliminated. The transformation of the E-Region magnitudes to the UBV system is: B = SP(g) - 0.07 SCI + 0.20 V = SP(v) + 0.08 SCI - 0.06 B-V = 0.85 SCI + 0.26 Whenever possible, the spectral types are from the Henry Draper Catalogue or its extension. Types for a large number of other stars were supplied by the Harvard College Observatory. G. G. Cillie classified many stars between -30deg. and -40deg. on plates taken at Bloemfontein. Three errors were discovered after the catalog was typed. These have been corrected in this version. 3558 For Co. D. 30d 5059. read 30d 5061 7726 For Co. D. 32d10484, read 32d10488 10580 For spectral type F8, read K0
Cape Photographic Catalog (CPC) data INDEX Index Number INDEX NUMBER ZONES (deg) ------------ ----------- 17A -30 to -35 18A -35 to -40 19A -52 to -56 20A -56 to -60 20B -60 to -64 21A -64 to -68 21B -68 to -72 21C -72 to -76 21D -76 to -80 22A -80 to -90 --- ID Catalog Identification Number --- rem Remark: a=supplemental star --- zone Durchmusterung Zone --- DM Durchmusterung Identification --- n_DM Remark on DM a = record has been inserted between successive DM numbers --- code Durchmusterung Code 20 = CD 40 = CpD --- RAh Right Ascension hours (1950.0) h RAm Right Ascension minutes min RAs Right Ascension seconds s DE- Declination sign (1950.0) --- DEd Declination degrees deg DEm Declination arcminutes arcmin DEs Declination arcseconds arcsec pmRA Centennial Proper Motion in RA cs/ha pmX Centennial Proper Motion RA*cos(DE) dam/ha pmDE Centennial Proper Motion in DE dam/ha Ep Epoch - 1900 a SPg Photographic Magnitude mag SPv Visual Magnitude mag CI Color Index mag Sp Spectral Type --- Julie Anne Watko SSDOO/ADC 1996 May 07 I_116.xml Elements of Minor Planets for 1986 1118 I/118 Elements of Minor Planets for 1986 Elements of Minor Planets for 1986 Yu V Batrakov Izdatel'stvo Nauka, Leningrad ??? ??? 1985 1985 I/124 : Elements of Minor Planets for 1987 I/127 : Elements of Minor Planets for 1988 Batrakov Yu.V. 1985, Elements of Minor Planets for 1986. Leningrad: Izdatel'stvo Nauka. Ephemerides Minor planets Osculating elements of minor planets numbered by November 1, 1984, are given. Perturbations by major planets were computed at the ITA of the USSR Academy of Sciences on a BESM-6 computer using programs by N.K. Sumzina and V.A. Shor.
Elements of minor planets for 1986 data ID Minor planet number --- Eq Equinox=1950.0 a Ep Epoch = 1986 06 19 (JED 2446600.5) a anom Mean anomaly --- peri Argument of perihelion --- node Node --- incl Inclination --- e Eccentricity --- mdm Mean daily motion --- mag Absolute magnitude of the planet B(1,0) mag code The nine-figure perturbation code A "1" in the i-th position of the code means that the perturbations from the i-th major planet had been taken into consideration when determining the elements. --- opp Number of oppositions for improvement --- N Number of observations for improvement --- obs_yr1 First year First and last year of the time interval covered by the observations used for improvement a obs_yr2 Last year a rms Mean-root square error Root-Mean-Square variation between observed and predicted positions. --- ref1 Code for the source of the elements MP = Minor Planet Circular EP = Ephemerides of Minor Planets --- ref2 Page or Year for source of the elements MP => page EP => year --- name Name or preliminary designation of planet --- aut Author of the elements --- date six-figure code of the date: YYMMDD Six-figure code of the date when the set of elements have been computed and written on tape at the ITA -- Julie Anne Watko SSDOO/ADC 1996 Aug 15 UNKNOWN UNKNOWN by exchange from the Moscow Data Center I_118.xml Bonner Sternverzeichniss, vierte Sektion, 1119 I/119 Southern Durchmusterung Bonner Sternverzeichniss, vierte Sektion, E Schoenfeld Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rheinischen Friedrich-Wilhelms-Universitat zu Bonn 8, Part IV 1886 ??? ??? Bonn: Adolph Marcus 1886 Surveys Durchmusterungen The Southern Durchmusterung (SD) was computerized at the Centre de Donnees Astronomiques de Strasbourg and at the Astronomical Data Center at the National Space Science Data Center, NASA/Goddard Space Flight Center. Corrigenda listed in the original SD volume and published by Kuestner and Sticker have been incorporated into the machine file. In addition, one star indicated to be "missing" in a published list, and later verified, is flagged so that it can be omitted from computer plotted charts if desired. Stars deleted in the various errata lists have been similarly flagged, while those with revised data are flagged and listed in a separate table. This catalog covers the zones -02 to -23 degrees.
The Southern Durchmusterung (SD, Schoenfeld 1886, Becker 1949, Schmidt 1967) is a visual survey of stars in the declination zones -02 to -23 degrees, completed as an extension to Argelander's (1859-62) monumental Bonner Durchmusterung (BD). Schoenfeld's survey was carried out using the same methods as had been used for the BD, which Schoenfeld had helped to compile as one of Argelander's assistants. The goal of the survey was to extend the BD to declination -23 deg (a plan originally adopted by Argelander) with approximately the same magnitude limits, although the primary instrument was of larger aperture (159 mm) than the 78-mm telescope used for the BD. Thus, whereas the BD magnitude estimates extend to 9.4 mag with all fainter stars assigned a magnitude of 9.5, the SD magnitude estimates extend to 9.9 mag with all fainter stars assigned a magnitude of 10. As with the BD, the SD contains a rather large number of stars fainter than 10.0 mag and even occasionally as faint as 11 mag. Positions are given to the nearest 0.1 sec in right ascension and 0.1 arcmin in declination as in the BD. The document originally prepared by the ADC (adc.doc) contains substantial additional information.
The SD catalog cat The catalog prefix --- zonesign The sign of the declination zone --- zone The declination zone deg num The number of the star within the zone --- n_num Code Upper and lower case codes. All lower case letters represent supplemental (footnoted) stars added to the catalog via published corrigenda. Upper case letters and asterisks are flags that indicate changes to the original data or to the status of a star in the catalog. They have the following meanings: * Data have been corrected as a result of corrigenda, or there are special notes associated with the star. All changes are given in Section A, Table 4, with appropriate notes. D The star has been deleted in a later edition of the catalog. This was done by overstriking entries with horizontal lines. M The star was noted as "missing" in a list published by Pickering (1907). This entry (there is only one such star) was verified by R. A. Downes and at the ADC. --- mag Estimated visual magnitude 20.0 = neb; 30.0 = var; 40.0 = nova or nova?; 50.0 = cum (integrated magnitude estimate of a cluster of stars). mag RAh Right Ascension 1855 (hours) h RAm Right Ascension 1855 (minutes) min RAs Right Ascension, 1855 (seconds) s DE- Sign of declination --- DEd Declination 1855 (degrees) deg DEm Declination 1855 (minutes) arcmin Changes from the printed cat. zone The SD zone --- num The SD number --- n_num Code on star number --- field The field changed --- old The printed value --- new The corrected value --- note Comments --- adc.doc The original document Nancy G. Roman NSSDC/ADC 1994 Nov 12 Drs. Warren and Ochsenbein express appreciation to M. J. Wagner, M. Maslo, and R. Bonnet, who keyed the SD data to disk at the CDS using preprocessing software written and implemented by F. Ochsenbein. They thank Dr. R. A. Downes for bringing the cases of "missing" BD and SD stars to their attention and are grateful for the support of the CDS director, Dr. C. Jaschek, during the course of the work. This document is based on the original ADC document prepared by Wayne Warren, Jr. of the ADC and Francois Ochsenbein of the CDS. UNKNOWN UNKNOWN The data in the machine-readable Southern Durchmusterung were keyed directly to disk storage from the published catalogs at the Centre de Donnees Astronomiques de Strasbourg (-02 through -21 deg. zones) and at the Astronomical Data Center of the National Space Science Data Center at the NASA Goddard Space Flight Center (-01, -22 and -23 deg. zones). Most of the data entry work was done at the CDS, where the data were also verified. The ADC zones -01 and -23, although not often used for stellar designations (the BD is used in zone -01 and the Cordoba Durchmusterung in zone -23), were added for completeness. The three ADC zones were computerized and proofread by Wayne Warren Jr. All zones were carefully examined, checked for sequencing and record counts, reformatted, and merged in the correct order at the ADC, where the final catalog was assembled. The published corrigenda lists were cross checked against the reprinted editions (1949, 1967) of the catalog. The final catalog was run through a verification program that checked numerical sequencing of the SD numbers, monotonic increase in right ascension, and allowed data ranges. All cases where stars are out of RA order were checked in the original data to verify that their positions are as in the original catalog or the corrigenda. The final file is ordered north to south strictly by SD number, i.e., in the zone order -01, -02, ..., -23. Users should note, however, that all stars are not strictly in right ascension order within each zone. This is because individual stars are occasionally out of RA order in the original catalog and because of corrections inserted from the corrigenda. UNKNOWN UNKNOWN All changes made to SD data and known to Warren and Ochsenbein were incorporated into the present machine-readable version. Unlike the Bonner Durchmusterung, where there had been numerous stars added and deleted, changes in supplemental entries from version to version, and a large number of data corrections, the changes to the SD are relatively few. There were two stars added as supplementary entries ("a" suffix), two stars deleted, and one star published as "missing" by Pickering (1907) and subsequently verified by R. A. Downes of Applied Research Corporation. A small list of corrections was also included in the introduction to the original published catalog. These modifications to the printed catalog are flagged by codes in byte 11 of the affected records and are listed in sdchg.dat. I_119.xml Common Proper Motion Stars In The AGK3 1121 I/121 Common proper motions stars in AGK3 Common Proper Motion Stars In The AGK3 J L Halbwachs Astron. Astrophys. Suppl. Ser. 66 131 1986 1986A&AS...66..131H Proper motions Stars, double and multiple The 326 common proper motion systems that have a ratio angular separation to proper motion smaller than 1000 years are in table1. The number of optical systems is expected to be around 4. Each system fills a 256 byte-length record that may also be considered as two 128 byte-length records for print-out edition. The 113 common proper motion systems that have a ratio angular separation to proper motion between 1000 and 3500 years are in table2. The number of physical systems is expected to be around 68. The presentation is the same as for table1. This table differs from the original printed version, since the the magnitude and the spectral type of the secondary component of the 47th system were corrected. The system 47 was also added to the notes.
Probability of 98.7% to be physical CPM Probability of 60% to be physical CPM Nseq sequential number of the system --- AGK2(A) number of the primary component --- HD/BD(A) HD or BD of the primary component --- ADS/IDS(A) ADS or IDS identification of the primary component --- Amag magnitude of the primary component mag n_Amag V when the magnitude is visual, P when it is photographic --- Sp(A) spectral type of the primary component --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin pm proper motion of the system mas/yr Id(A) other identification: Luyten Double Star (LDS) or cluster member --- Notes Note codes (see Notes sections below) --- AGK2(B) AGK2 number of the secondary component --- HD/BD(B) HD or BD of the secondary component --- ADS/IDS(B) ADS or IDS identification of the secondary component --- Bmag magnitude of the secondary component mag n_Bmag V when the magnitude is visual, P when it is photographic --- Sp(B) spectral type of the secondary component --- PA position angle of the secondary component deg Dist angular separation between the components arcsec rho/mu Ratio angular separation to proper motion, in 1000 years. kyr Id(B) Other identification of the secondary component --- CDS Catalogue Service CDS 1994 Oct 06 I_121.xml Bonner Durchmusterung 1122 I/122 Bonner Durchmusterung Bonner Durchmusterung F W A Argelander Bonner Sternverzeichniss, erste bis dritte Sektion, Astronomischen Beobachtungen auf der Sternwarte des Koeniglichen Rheinishen Friedrich-Wilhelms-Universitaet zu Bonn, Baende 3-5, ??? ??? 1859-62 I/119 : Southern part "Suedlicher Durchmusterung" (-02 to -23 degrees) I/114 : Cordoba Durchmusterung (-22 to -90 degrees) I/108 : Cape Photographic Durchmusterung (-18 to -90 degrees) Argelander, F. W. A. 1859-1862, Bonner Sternverzeichniss, erste bis dritte Sektion, Astronomischen Beobachtungen auf der Sternwarte des Koeniglichen Rhein., Friedrich-Wilhelms-Universitat zu Bonn, Bande 3-5. Becker, F. 1951, Bonner Durchmusterung, Noerdlicher Teil, Deklinations-Zonen -1 bis +89 grade Sternverzeichnis, dritte, berichtigte Auflage (Bonn: Ferd. Duemmlers Verlag). Chandler, S. C. 1896, Astron. J. 16, 145. Couteau, P., Fulconis, M., Ochsenbein, F., Wagner, M. J., and Maslo, W. 1983, Inf. Bull. CDS No. 25, p. 83. Giclas, H. L., Burnham, R. Jr., and Thomas, N. G. 1971, Lowell Proper Motion Survey, Northern Hemisphere, The G Numbered Stars (Flagstaff: Lowell Observatory). Kuestner, F. 1903, Bonner Durchmusterung des Noerdlichen Himmels, zweite berichtigte Auflage, Bonn Universitats Sternwarte (Bonn: A. Marcus und E. Weber's Verlag). Kuestner, F. 1908, Astron. Nach. 178, 33 (Nr. 4251). Kuestner, F. 1918, Astron. Nach. 206, 69 (Nr. 4929). Kuestner, F. 1925, Astron. Nach. 223, 309 (Nr. 5347). Luyten, W. J. 1979, 1980, New Luyten Catalogue of Stars with Proper Motions Larger than Two Tenths of an Arcsecond (Minneapolis: University of Minnesota). Luyten, W. J. and Hughes, H. S. 1980, Proper Motion Survey with the Forty- Eight Inch Schmidt Telescope. LV. First Supplement to the NLTT Catalogue (Minneapolis: University of Minnesota). Pickering, E. C. 1885, Harv. Ann. 14. Pickering, E. C. 1892, Harv. Ann. 23. Pickering, E. C. 1907, Astron. Nach. 175, 139. Pickering, E. C. 1913, Harv. Ann. 72. Schmidt, H. 1968, Bonner Durchmusterung, Noerdlicher Teil, Deklinations-Zonen -1 bis +89 grade Sternverzeichnis, vierte Auflage (Bonn: Ferd. Duemmlers Verlag). Sticker, B. 1935, Astron. Nach. 256, 341 (Nr. 6139). Sticker, B. 1936, Astron. Nach. 259, 187 (Nr. 6203). Sticker, B. 1938, Astron. Nach. 265, 127 (Nr. 6344). Upgren, A. R., Grossenbacher, R., Penhallow, W. S., MacConnell, D. J., and Frye, R. L. 1972, Astron. J. 77, 486. Wagner, M. J. 1984, Inf. Bull. CDS No. 26, p. 87. Wagner, M. J. 1986, Inf. Bull. CDS No. 30, p. 117. Warren, W. H. Jr. 1987, Inf. Bull. CDS No. 32, p. 67. Warren, W. H. Jr. and Kress, K. 1980, Astron. Data Center Bull. 1, 19. Surveys Durchmusterungen The Bonner Durchmusterung (BD, Argelander 1859-62, Kuestner 1903, Becker 1951, Schmidt 1968) is a visual survey of stars in the declination zones +89 to -01 degrees. The goal of the survey was to obtain a position and estimated visual magnitude for every star visible with the 78-mm Bonn telescope. Actual magnitude estimates were made and reported to 0.1 mag for all stars down to 9.5 mag, with fainter stars being assigned to 9.5. Positions are given to the nearest 0.1 sec in right ascension and 0.1 arcmin in declination.
The Bonner Durchmusterung (BD, Argelander 1859-62, Kuestner 1903, Becker 1951, Schmidt 1968) is a visual survey of stars in the declination zones +89 to -01 degrees performed by allowing the telescope to drift along the mean declination of each zone and recording the positions and magnitudes of stars crossing the transit line of each field. Actual magnitude estimates were made and reported to 0.1 mag for all stars down to 9.5 mag, with fainter stars being assigned to 9.5. The BD actually contains a rather large number of stars fainter than 10.0 mag. Positions are given to the nearest 0.1 sec in right ascension and 0.1 arcmin in declination. The catalog includes all corrigenda published in the original BD volumes have been incorporated into the machine file, along with changes published by Kuestner and Sticker following the 1903 edition. In addition, stars indicated to be "missing" in published lists and verified by various techniques are flagged so that they can be omitted from computer plotted charts if desired. Stars deleted in the various errata lists have been similarly flagged, while those with revised data are flagged and listed in a separate table. No other corrections or changes have been incorporated into the original data, e.g., from more modern positions and magnitudes or from comparison with other catalogs. The original document (adc.doc) contains substantial additional information.
The Bonner Durchmusterung catalog cat The catalog prefix --- zonesign The sign of the declination zone --- zone The declination zone deg num The number of the star within the zone --- suppl Note a, b, or c: star is added in the 1903 or later editions * Data have been corrected as a result of corrigenda ? Existence of the star by Kuestner or Sticker D The star was deleted in a later edition by overstriking M The star was noted as missing by Chandler or Pickering --- mag Estimated visual magnitude 20.0 = neb; 30.0 = var; 40.0 = nova or nova?; 50.0 = integrated magnitude for a cluster mag RAh Right Ascension 1855 (hours) h RAm Right Ascension 1855 (minutes) min RAs Right Ascension, 1855 (seconds) s DE- Sign of declination --- DEd Declination 1855 (degrees) deg DEm Declination 1855 (minutes) arcmin Changes since the original printing zone The BD zone --- num The BD number --- suppl Supplemental designation --- field The field changed --- old The printed value --- new The corrected value --- note Comments 1 Star of approximately 13 mag at nominal position. 2 There is a "?" in the 1903 edition. No star could be found on the POSS prints or on the Vehrenberg Atlas Stellarum chart. 3 Star of approximately 12 mag at nominal position. 4 Candidate in field, but it is 3 arcmin north of the BD position. Star listed by Upgren et al. (1972) at right ascension an hour away from the BD position. 5 Faint star(s) in field, but "M" flag retained in record. 6 Possible variability noted by Kuestner (1918). 7 Existence also questioned by Kuestner (1908). 8 There is a "?" in the 1903 edition that was later removed by Kuestner (1918). 9 There is a "?" in the 1903 edition of the BD. 10 Non-BD star within 10 arcmin of nominal BD position. 11 Non-BD star within 10 arcmin of nominal BD position; existence questioned by Kuestner. 12 Non-BD star within 10 arcmin of nominal BD position. There is a "?" a "?" in the 1903 edition of the BD. 13 There is a question mark in the 1903 edition that was later removed by Kuestner (1918). There is a non-BD star within 10' of nominal BD position. --- adc.doc The original document Nancy G. Roman NSSDC/ADC 1994, modified CDS 20-Sep-1995 Nov 12 This immense project was successfully completed only through the combined efforts of the institutes and individuals listed above and the work of many persons within those institutes. The initial work at the Astronomical Data Center/NSSDC was begun and supervised by Drs. J. M. Mead, T. A. Nagy, and Wayne Warren, Jr. but the punching could never have been begun, nor the project completed without the support of the former NSSDC Director, Dr. James I. Vette. This support continued under Dr. James L. Green, and the Head of NSSDC's Central Data Services Facility, Dr. Joseph H. King. The NSSDC zones (+19 to -01 ) were punched by Beth Alexander, Carol Bergstrom, and Margy Goodwin, while monitoring software for data transfer was written by Frank Barnes and migration to magnetic tape was done by Charleen Perry under the supervision of Ralph Post. ADC software for the formatting of binary data and for the exact reproduction of published pages for proofreading was written by Wayne Warren Jr. but the actual proofing was accomplished by summer students Paula Feldman and Kimberly Kniffen, who also assisted greatly with error checking, recording, and data corrections. Zones +24 and +25 were keyed directly to disk, printed, and proofread by Warren, while B. N. Rappaport arranged for the keypunching of zones +23 to +20 by Syntronix, Incorporated, of Sherman Oaks, California, checked the data with his own computer programs and financed the work himself. The punching of zones +59 to +26 was accomplished at l'Observatoire de Nice by M. Fulconis, under the direction of P. Couteau, and their proofreading was done at the CDS by M. J. Wagner and W. Maslo. Zones +80 to +60 were keyed directly to disk at the CDS by M. J. Wagner, W. Maslo, and R. Bonnet, with preprocessing software written and implemented by F. Ochsenbein. Zones +25 and +24 were also computerized at the CDS and used to check the data prepared at the Astronomical Data Center. Finally, the compilers thank Dr. R. A. Downes of Applied Research Corporation for bringing the "missing" stars to our attention, for supplying a complete list of the stars, and for rechecking certain questionable cases. This document is based on the original ADC document prepared by Wayne Warren Jr. UNKNOWN UNKNOWN The data in the machine-readable Bonner Durchmusterung were keypunched directly from the published catalogs through the collaborative efforts of personnel at l'Observatoire de Nice, the Centre de Donnees Astronomiques de Strasbourg, the National Space Science Data Center at the NASA/Goddard Space Flight Center, and with the help of B. N. Rappaport, then at the NASA Jet Propulsion Laboratory. The following is the distribution of the work: Zones Location +89 to +60 Centre de Donnees Astronomiques de Strasbourg (CDS) +59 to +26 L'Observatoire de Nice +25 to +24 National Space Science Data Center (also CDS) +23 to +20 B. N. Rappaport (+23 also done at CDS) +19 to -01 National Space Science Data Center (+14 also done at Nice) Zones +89 to +60 were also verified at the CDS and zones +59 to +26 were proofread there, while the remaining zones were proofread at the Astronomical Data Center. Redundant zones were compared by computer and appropriate corrections were made. All zones were carefully examined, checked for sequencing and record counts, reformatted, and merged in the correct order at the ADC, where the final catalog was assembled. The supplemental entries were incorporated into the ADC/NSSDC and Rappaport zones from an earlier catalog prepared by Warren and Kress (1980) or used to check existing supplemental entries in the Nice and CDS zones. The published corrigenda lists were cross checked extensively against the reprinted editions of the catalog for preparation of the tables in the appendix of this document. Apparent discrepancies were checked on the BD charts and on the prints of the Vehrenberg Atlas Stellarum. The final catalog was run through a verification program that checked numerical sequencing of the BD numbers, monotonic increase in right ascension, and allowed data ranges. All cases where stars are out of RA order were checked in the original data to verify that their positions are as in the original catalog. The final file is ordered north to south strictly by BD number, i.e., in the zone order +89; +88; ...; -01. Users should note, however, that all stars are not strictly in right ascension order within each zone. This is because individual stars are occasionally out of RA order in the original catalog and because of corrections inserted from the corrigenda. Thus, if the machine catalog is sorted by increasing RA, e.g., for search purposes, some BD numbers will become disordered. *(20-Sep-1995, F. Ochsenbein, at CDS): Three further corrections made on stars: BD+65 820 (was named BD+65 821), BD+65 821 (was named BD+65 821!). BD-00 1000 (a digit was missing in the DEm field) I_122.xml Lunar Occultations of IRAS Point Sources, 1986-1990 1123 I/123 Lunar Occultations of IRAS Point Sources, 1986-1990 Lunar Occultations of IRAS Point Sources, 1986-1990 M Simon L Cassar W P Chen Astrophys. J. Suppl. Ser. 62 673 1986 1986ApJS...62..673S Infrared sources Occultations The Lunar Occultations of IRAS Point Sources lists objects in the IRAS Point Source Catalog that were occulted by the Moon during 1986-1990.
The occultation predictions were based on the formulae for the lunar ephemeris developed by Van Flandern and Pulkinnen (1979). The topocentric predictions from this code are accurate to about +/-30s.
Data IRAS IRAS Point Source Cat. Object Name --- yr1 Starting Year yr1 and yr2 are the starting and ending years of the interval during which geometric events occur for the object. Some of the objects for which the ending year indicated is 1990 may actually have events in subsequent years because times later than 1990 were not considered in the present work. For objects having two intervals during 1986-1990 in which geometric events occur, the second interval is indicated in the line following the first entry. a yr2 Ending Year yr1 and yr2 are the starting and ending years of the interval during which geometric events occur for the object. Some of the objects for which the ending year indicated is 1990 may actually have events in subsequent years because times later than 1990 were not considered in the present work. For objects having two intervals during 1986-1990 in which geometric events occur, the second interval is indicated in the line following the first entry. a flux12 Mantissa for 12 um Flux Density flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. Jy exp12 Exponent for 12 um Flux Density exp fields list the exponent of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. --- flux25 Mantissa for 25 um Flux Density flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. Jy exp25 Exponent for 25 um Flux Density exp fields list the exponent of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. --- flux60 Mantissa for 60 um Flux Density flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. Jy exp60 Exponent for 60 um Flux Density exp fields list the exponent of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. --- flux100 Mantissa for 100 um Flux Density flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. Jy exp100 Exponent for 100 um Flux Density exp fields list the exponent of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. --- q_flux12 Quality of flux12 flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. q_flux fields refer to the flux-quality flags at 12, 25, 60 and 100 um, as indicated in the IRAS Point Source Catalog: H = high-quality detection M = medium-quality detection U = upper bound --- q_flux25 Quality of flux25 flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. q_flux fields refer to the flux-quality flags at 12, 25, 60 and 100 um, as indicated in the IRAS Point Source Catalog: H = high-quality detection M = medium-quality detection U = upper bound --- q_flux60 Quality of flux60 flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. q_flux fields refer to the flux-quality flags at 12, 25, 60 and 100 um, as indicated in the IRAS Point Source Catalog: H = high-quality detection M = medium-quality detection U = upper bound --- q_flux100 Quality of flux100 flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. q_flux fields refer to the flux-quality flags at 12, 25, 60 and 100 um, as indicated in the IRAS Point Source Catalog: H = high-quality detection M = medium-quality detection U = upper bound --- cat Catalog Number For an object for which an identification with an object listed in some other astronomical catalog is provided in the IRAS Point Source Catalog, the catalog number, following the conventions of the IRAS Point Source Catalog, is given. --- name Object Name in Other Catalog For an object for which an identification with an object listed in some other astronomical catalog is provided in the IRAS Point Source Catalog, the first object name, following the conventions of the IRAS Point Source Catalog, is given. --- rem Remark An asterisk appears where there is more than one identification with an object listed in another astronomical catalog. Only the first is indicated in cat and name. The rest may be obtained from the original catalog. --- Julie Anne Watko SSDOO/ADC 1996 Feb 09 We thank Dr. Simon for forwarding this catalog to the ADC. I_123.xml Combined Lick-Voyager Reference Star Catalogue. 1125A I/125A Combined Lick-Voyager Reference Star Catalogue Combined Lick-Voyager Reference Star Catalogue. D W Dunham Unpublished ??? ??? 1986 1986 Positional data The catalogue contains accurate equatorial coordinates for stars in several bands of sky against which cameras of Voyager spacecraft were pointed for observations in the regions of Jupiter, Saturn, Uranus and Neptune during the flyby. This catalogue is compiled by combining the four reference star catalogues for Voyager mission: Uranus-Voyager Reference Star Catalogue <I/115> Klemola A.R., Owen Jr. W.M. <Lick Obs., Jet Propulsion Lab. (1985)> Neptune-Voyager Reference Star Catalogue <I/140> Klemola A.R., Owen Jr. W.M. <Lick Obs., Jet Propulsion Lab. (1986)> Jupiter-Voyager Reference Star Catalogue <I/152> Klemola A.R., Morabito L., Taraji H. <Lick Obs. (1978)> (Corrections by Owen Jr. W.M., 1990) Saturn-Voyager Reference Star Catalogue <I/153> Klemola A.R., Taraji H., Ocampo A. <Lick Obs. (1979)> (Corrections by Owen Jr. W.M., 1990) Note however that the corrections applied in 1990 to the last two catalogue Jupiter-Voyager and Saturn-Voyager are not incorporated here.
The Catalogue DMsign DM zone sign, or Lick indicator: + or - : Bonner Durchmusterung C : Cordoba Durchmusterung L : Lick (non-DM) --- DMzone DM zone (without sign), or if Lick: 1=Jupiter, 2=Saturn, 3=Uranus-pre, 4=Uranus-post, 5=Neptune --- DMnum sequence number in DM (or Lick) zone --- Vmag V magnitude (in unit of 0.01mag.) 0.01mag RAh Right Ascension B1950 (hours) at Epoch h RAm Right Ascension B1950 (minutes) min RAms Right Ascension B1950 (seconds) ms pmRA proper motion in RA (0.001s/century) 0.01ms/a DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) at Epoch deg DEm Declination B1950 (minutes) arcmin DEcs Declination B1950 (0.01 seconds) 10mas pmDE proper motion in DE (0.01arcseconds/cent) 0.1mas/a Bmag B magnitude (0.01mag.) 0.01mag SCnum Lick source number, see remarks below. --- SAO SAO number <I/131> --- SpType spectral type (if given) --- e_RA error of RA (0.01arcseconds) 10mas e_pmRA error of pmRA (0.01arcseconds/century) 0.1mas/a e_DE error of DE (0.01arcseconds) 10mas e_pmDE error of pmDE (0.01arcseconds/century) 0.1mas/a Epoch epoch of RA and DE, 0.01years since 1900. 0.01a plx parallax (0.0001arcseconds) 0.1mas AGK3 AGK3 designation (zone in bytes 81-83, number in bytes 85-88) --- Francois Ochsenbein CDS 1995 Nov 02 UNKNOWN UNKNOWN * Catalogue provided by ADC, NASA/GSFC * 16-Jul-1993: RA and DE transformed by Dr K. Nakajima (Visiting Astronomer at CDS) * 30-Aug-1993: Errors communicated by S. Nishimura, Tokyo Data Centre: The star names in BD +1 zone are erroneous: for read + 1 0 +14 1641 + 1 0 +19 1769 + 1 0 +19 1805 + 1 0 +26 1677 + 1 1528 +21 1528 + 1 1596 +21 1596 + 1 1643 +19 1643 + 1 1725 +14 1725 + 1 1792 +23 1792 + 1 1793 +18 1793 Note also that there are two stars named "L 1 1". * 02-Nov-1995: The corrections mentioned above by S. Nishimura have been incorporated into 'A' version, as well as the following modifications (Francois Ochsenbein, CDS): => The second "L 1 1" was changed to "L 4 1" => The zone sign of AGK3 numbers were transformed into '+' and '-' (instead of 'N' and 'S') => All southern DM numbers were erroneously indicated 'C' (from Cordoba Durchmusterung); 'C' was replaced by '-' (Bonner Durchmusterung) when appropriate. UNKNOWN UNKNOWN (David Dunham, 1986 Oct. 16): E-terms have been added to the Uranus catalogs, so that these are included for all stars. In column 47-51, SCnum, the number is the sequential number if actual DM No.'s (not "L" in column 1) are in columns 1-8. This is also the case for Neptune catalog stars, for which no plate or other catalog ID's are available. Otherwise, an abbreviation of the Lick plate No. is in column 47-48, and the No. of the star on the plate in column 49-51, both right-justified (as are all "I n" fields). "9999" in B-mag. field means no B-mag. is available. SAO-only and AGK3-only stars in the Uranus catalogs, which were not on any Lick plate, were skipped. Stars in the Uranus-Gemini catalog were matched with the Jupiter catalog; for matched stars, Uranus data superseded Jupiter data whenever possible (Jupiter data was used in the construction of the Uranus-Gemini catalog at J.P.L.). For 16 of the matched stars, one catalog gave an AGK3 No. and the other didn't. 173 stars in the Uranus-Sagittarius catalog had no magnitude informations; I arbitrarily set V-mag. for these stars = 11.4, unless the star was in the Co.D., in which case, I set V-mag. = 10.4. Although the position information in the Neptune catalog should be good, it has not been cross-referenced to other catalogs, and the photometry has not been calibrated. What I have is a preliminary version sent by Arnold Klemola to me early in September. Unlimited distribution of the Neptune catalog needs to wait until more work is done on it. In the meantime, any further distribution of Neptune catalog data needs Klemola's approval, although I am confident that this will be readily granted for those using the catalogs for occultations. David Dunham 1986 Oct. 16 I_125A.xml Photographic Observations of Visual Double Stars 1128 I/128 Photographic Obs. Visual Double Stars Photographic Observations of Visual Double Stars E van Albada-van Dien E Panjaitan Astron. Astrophys. Suppl. 68 117 1987 1987A&AS...68..117V Stars, double and multiple This catalog contains the results of photographic observations of 248 double stars, obtained at the Bosscha Observatory at Lembang, Indonesia 1981-1983.
Photographic obs. of visual double stars RAh Right Ascension (1900,2000) hours Where bytes 1-54 are blank, bytes 55-127 belong to the previous record. h RAdm19 Right Ascension (1900) deciminutes dmin RAdm20 Right Ascension (2000) deciminutes dmin DE- Declination (1900,2000) sign --- DEd Declination (1900,2000) degrees deg DEm19 Declination (1900) arcminutes DEd applies to both epochs of DEm. DEm values greater than 60 arminutes result. These do not indicate errors in the data. arcmin DEm20 Declination (2000) arcminutes DEd applies to both epochs of DEm. DEm values greater than 60 arminutes result. These do not indicate errors in the data. arcmin rem Remark * = Pair has been removed from the program --- ADS ADS number or name mentioned in IDS --- paren1 Parentheses --- mag1 Magnitude of primary component from IDS blank = Null 99.9 = Variable mag comma Comma separator --- mag2 Magnitude of secondary component from IDS blank = Null 99.9 = Variable mag Sp Spectral type from IDS --- Ep Mean Epoch of observations - 1900 a dRAcosDE Mean value of delta(RA) * cos(DE) arcsec e_dRAcosDE Standard error of delta(RA) * cos(DE) Standard errors are given in units of the last decimal given. --- dDE Mean value of delta(DE) arcsec e_dDE Standard error of delta(DE) Standard errors are given in units of the last decimal given. --- D Distance derived arcsec e_D Standard error of D Standard errors are given in units of the last decimal given. --- PA Position Angle at Ep deg e_PA Standard error of PA Standard errors are given in units of the last decimal given. --- nplates Number of plates --- nimages Number of images blank = Null 99.9 = Variable --- paren2 Parentheses --- Wt Sum of weights --- paren3 Parentheses --- note Notes N = Northern Declination --- Julie Anne Watko SSDOO/ADC 1996 May 10 I_128.xml A survey of trigonometric parallaxes and proper motions with the UK Schmidt telescope - II. Astrometric and photometric data for a complete sample of 6125 stars brighter than B=17.5, V=17.0 in the South Galactic Cap. 1129 I/129 Parallaxes and Proper Motions near SGP A survey of trigonometric parallaxes and proper motions with the UK Schmidt telescope - II. Astrometric and photometric data for a complete sample of 6125 stars brighter than B=17.5, V=17.0 in the South Galactic Cap. C A Murray R W Argyle P M Corben Mon. Not. R. Astron. Soc. 223 629 1986 1986MNRAS.223..629M J/AJ/103/514 : (I colour and spectroscopic observations of the stars) Galactic pole, south Parallaxes, trigonometric Proper motions Regional catalog The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V. Nomenclature Notes: The stars from this catalogue are named "RGO" followed by the number in "RGO" column of "catalog" file.
The Catalogue Seq Running Number --- RGO Serial number in RGO files --- Bmag (photographic) mag Vmag (photographic) mag B-V (photographic) mag q_RGO Astrometric quality code number=1 The quality code is blank for satisfactory data; it takes otherwise the following basic values 1 : Abnormal errors in Series B 2 : Abnormal errors in Series A 4 : Inconsistent results between the two Series The remaining codes are combinations of these (e.g. 3 = 1 + 2) --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec pmX Proper motion in X ("/y) arcsec/a pmY Proper motion in Y ("/y) arcsec/a plx Trigonometric parallax (") arcsec e_pos Internal standard error of a position coordinate arcsec e_pm Internal standard error of a proper motion component (pmX or pmY) arcsec/a e_plx Internal standard error of trigonometric parallax (plx) arcsec Epoch Mean epoch of observation a chi2 Chi-squared (5 degrees of freedom) from combination of Series A and B --- Xpos Standard coordinate X referred to RA= 0h 53m, Dec=-28.0deg (B1950) arcmin Ypos Standard coordinate Y referred to RA= 0h 53m, Dec=-28.0deg (B1950) arcmin Rem An asterisk (*) in this column signifies a further identification in Table 9 --- Francois Ochsenbein CDS 1995 Nov 02 We sincerely thank Drs C.A. Murray and R. Martin for having provided the magnetic tape version to CDS in November 1986. UNKNOWN UNKNOWN * November 1986: Tape provided by C.A. Murray (RGO) to CDS * 29-Jun-1993: First standardized description at CDS I_129.xml The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI 1130 I/130 LDS Catalogue: Doubles with Common Proper Motion The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1969 1969PMMin..21....1L The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1970 1970PMMin..25....1L The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1972 1972PMMin..29....1L The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1975 1975PMMin..40....1L The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1977 1977PMMin..50....1L The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1980 1980PMMin..55....1L The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1983 1983PMMin..64....1L The LDS Catalogue: Double Stars with Common Proper Motion Proper motion survey with the 48-inch Schmidt Telescope, XXI W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1987 1987PMMin..71....1L Proper motions Stars, double and multiple This catalogue contains all double stars with common proper motion discovered by Luyten since 1940 up to 1987 (references below). When Luyten had noticed that an entry was duplicated (ref. 8 and 9), only the former LDS number was kept in the data file but with the data given for the latter. The unique exception is LDS 6166, which is a duplicate of LDS 5662, but with an additional component. The systems classified as optical by Luyten were also rejected from the main data files. All the rejected data were put together in a separate file. All coordinates are for the equinox 1950; when the original publication gave another equinox (this is the case for ref. 1), the 1950-coordinates were calculated. The catalogue contains all the systems, sorted by increasing LDS numbers. Duplicate entries and optical systems listed by Luyten were rejected. The catalogue contains 6121 systems, including 87 triple and 1 quadruple systems. The number of records is thus 6210, since each triple system occupies 2 records and the quadruple system 3.
The Catalogue Data rejected for duplicate numbers or optical systems LDS LDS number number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- Mult 't' indicates a system is triple and 'q' it is quadruple. Then, the LDS number is the same for all entries. number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- RAh Right Ascension 1950 (hours) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. h RAm Right Ascension 1950 (minutes) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. min RAs Right Ascension 1950 (seconds) number=1 When the seconds are provided, the RAm fractional part is blank s DE- Declination 1950 (sign) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- DEd Declination 1950 (degrees) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. deg DEm Declination 1950 (minutes) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. arcmin mR1 Photographic R magnitude of the primary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mR1 Uncertainty flag on mR1 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mB1 Photographic magnitude of the primary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mB1 Uncertainty flag on mB1 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- color1 Color class of the primary component number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mR2 photographic R magnitude of the secondary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mR2 Uncertainty flag on mR2 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mB2 photographic magnitude of the secondary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mB2 Uncertainty flag on mB2 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- color2 Color class of the secondary component number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- pm Annual proper motion, number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. arcsec/a pmPA Direction (N to E) of the proper motion number=2 LDS 3543 has a value of 403deg (outside standard limits) deg Theta Position angle, see also Quadrant number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) deg Sep Separation between components number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) arcsec Quadrant Quadrant designation for ref.1 number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) --- Remark Short remark and/or other identification number=3 the reasons for rejection are in bytes 81-91 in file "reject". A '*' refers to a remark (see 'Individual Remarks' below) The {Lambda} identifications given in ref.1 were not keypunched. --- Ref Reference code (see References section) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- J.-L. Halbwachs, F. Ochsenbein CDS 1997 Feb 04 UNKNOWN UNKNOWN Keypunched at CDS in 1987 * 15-Jun-1994: Corrected a few errors (existing in the publication) LDS 3593: third decimal place of proper motion (pm) set to blank LDS 4309: "+" embedded in DEm LDS 4871: RAm was -1 LDS 5644: secondary magnitudes were 18.,0 19.1 LDS 5679: third decimal place of proper motion (pm) set to blank LDS 5999: third decimal place of proper motion (pm) set to blank * 04-Feb-1997: ReadMe file standardized, and disentangled Quadrant from Theta values in data files * 19-Sep-1997: a few bad magnitude values (above 90.0) corrected in both main and rejected files. I_130.xml A New List of Trapezium-Type Multiple Systems 1134 I/134 A New List of Trapezium-Type Multiple Systems A New List of Trapezium-Type Multiple Systems G N Salukvadze Byull. Abastumani Astrofiz. Obs. No. 49, pp. 39-68 ??? ??? 1978 1978AbaOB..49...39S Stars, double and multiple This catalogue is based on the following works: 1 - G.N.Salukvadze, Abastumanskaya Astrofiz.Obs., Bull.49,39 (1978): A new list of trapezium-type multiple systems. and 2 - G.N.Salukvadze, Astrofizika 14 (1), 57 (1978): The catalogue of trapezium-type multiple systems. This catalogue of trapezium-type multiple systems was compiled on the basis of the index-catalogue of visual binary stars (IDS) (Jeffers et al., 1963). At the period of compilation of the Abastumani Catalogue, the IDS was the most complete catalogue concerning not only stars, but also the data on double stars. Besides giving relative positions, the IDS presents the coordinates at 1900 and 2000 epochs, as well as in most cases magnitudes, spectral classes and proper motions. The IDS contains all double and multiple stars from the North to the South poles with relative positions published up to the end of 1960, their total number being 64247. In order to select optimum value of K (ratio of the largest to the smallest distances among the components), which is the main criterion for relating a multiple star to the trapezium type, the dependence of the observed trapezia number on the K value has been analysed, and the value 2.6 adopted for it. To exclude optical components, upper limits for the distances of faint components to the main star have been introduced, and the components fainter than 12.5 mag. were excluded altogether (Salukvadze, 1978). The catalogue of trapezium-type multiple systems contains 412 trapezia, for which spectral classes in the MK system have been specified, after examining all main spectral catalogues (Jaschek et al., 1964; Kennedy et al., 1974; Hauck et al., 1975; Cruz-Gonzales et al., 1974; Lindsey et al., 1968). This was done for 100 systems, including 65 stars of O and B spectral classes. The following data on trapezia are given in the catalogue: positional angles and distances, magnitudes and spectral classes according to HD as well as MK, and the ADS and BD identification number of the main star. On the basis of the probability, deduced by Ambartsumian (1954), the number of pseudotrapezia was estimated, that is, the number of multiple stars, which in fact have no trapezium-type configurations, but are observed as trapezia as a result of their projection on the celestial sphere. The number of estimated pseudo-trapezia is 167. It should be mentioned that among 59 trapezia, the main components of which are of the O-B2 spectral class, there are only 5 pseudotrapezia. This enables us to maintain that there is a considerable percentage of real trapezia among the ones of mentioned spectral classes. Evaluation of the number of optical systems, formed as a result of the appearance of background stars in circles, which are determined by the upper limits of components' distances, led to their insignificant number - 9. The main star of the trapezium-type multiple system generally occupies 72 bytes and is marked by an asterisk (*) in the first and 72nd bytes. For each component of multiple systems 72 bytes were also taken, but, unlike the main star, the component's record is not marked by an asterisk (*), and the data for it is contained in bytes 17-39, which are: designation of components, relative positions and magnitudes of stars in trapezia.
Main catlog main1 Denotes a main star --- N Ordinal number --- RAh1900 RA Hours (1900.0) h RAm1900 RA Minutes (1900.0) This field is listed to an accuracy of 0.1 minutes of time. 0.1min DE-1900 Dec Sign (1900.0) This field uses the uncommon values N-NORTH, S-SOUTH instead of + or -. --- DEd1900 Dec Degrees (1900.0) deg DEm1900 Dec Minutes (1900.0) The values are in arcminutes according to the IDS Catalogue. Sometimes these values are greater than 60. arcmin comp Designation of components --- PA Positional angle of a component relative to the main star deg sep Distance of a component to the main star arcsec Mvmain Magnitudes of the main star mag Mvcomp Magnitudes of trapezium components mag SpIDS Spectral class of the main star according to IDS --- SpMK Spectral class of the main star in the MK system --- ADS ADS number --- DM Durchmusterung number --- main2 Denotes a main star --- James E. Gass SSDOO/ADC 1997 Jul 30 The author thanks professor V.A.Ambartsumian for valuable advice during the compilation of the catalogue of trapezium-type multiple systems, As well as his collaborators from the Abastumani Astrophysical Observatory M. Butikashvili and N. Kiselyova for the transfer of the Trapezia Catalogue on magnetic tape. I_134.xml Lunar Occultations of IRAS Point Sources: 1991-2000 1142 I/142 Lunar Occultations of IRAS Point Sources 1991-2000 Lunar Occultations of IRAS Point Sources: 1991-2000 M Simon L Cassar W P Chen Astrophys. J. Suppl. Ser. 69 651 1989 1989ApJS...69..651C I/123 : Lunar Occultations of IRAS Point Sources, 1986-1990 IRAS Point Source Catalog. 1985, Joint IRAS Science Working Group (Washington, DC: GPO). Cassar L., Chen W.P. and Simon M. 1989, Astrophys. J. Suppl. Ser. 69, 651. Simon M., Cassar L. and Chen W.P. 1986, Astrophys. J. Suppl. Ser. 62, 673. Occultations Infrared sources A listing of objects in the IRAS Point Source Catalog (1985) that were or will be occulted by the Moon during 1991-2000 is presented. Objects from the IRAS PSC that will have geocentric occultations during the years 1991- 2000 were identified using procedures described in Simon et al. (1986). This list is a sequel to the list of occultations for the years 1986-1990 (ADC catalog 1123).
Occultation data on IRAS PSC objects IRAS IRAS Point Source Cat. Object name If IRAS is blank, then record is a continuation for the star in the previous record. --- yr1 Beginning year a yr2 Ending year a flux12 12 um Flux density Jy flux25 25 um Flux density Jy flux60 60 um Flux density Jy flux100 100 um Flux density Jy q_flux12 Quality flag on flux12 H = high-quality detection M = medium-quality detection U = upper bound --- q_flux25 Quality flag on flux25 H = high-quality detection M = medium-quality detection U = upper bound --- q_flux60 Quality flag on flux60 H = high-quality detection M = medium-quality detection U = upper bound --- q_flux100 Quality flag on flux100 H = high-quality detection M = medium-quality detection U = upper bound --- cat Catalog number For an object for which an identification with an object listed in some other astronomical catalog is provided in the IRAS PSC, the catalog number, following the conventions of the IRAS PSC, is given in the cat field, and the object name in that catalog is given. Where there is more than one identification with an object listed in another astronomical catalog, an asterisk (*) appears in rem. In this case, only the first identification is indicated in cat and ID. The rest may be obtained from the original IRAS PSC. --- ID Star identification in cat --- rem Remark on multiple identifications --- Julie Anne Watko SSDOO/ADC 1996 Aug 21 I_142.xml Fourth Fundamental Catalogue and Supplement 1143 I/143 Fourth Fundamental Cat and Suppl Fourth Fundamental Catalogue and Supplement W Fricke A Kopff Veroeff. Astron. Rechen-Inst., Heidelb., No. 10 ??? ??? 1963 1963VeARI..10....1F Fourth Fundamental Catalogue and Supplement W Fricke A Kopff Veroeff. Astron. Rechen-Inst., Heidelb., No. 11 ??? ??? 1963 1963VeARI..11....1F I/149 : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) Extension (Fricke+ 1991) Positional data Proper motions Fundamental catalog Stars, fundamental The FK4 was an attempt to establish a fundamental system of stellar positions and proper motions for the 1950 equinox using as much position data as were available. Most of the stars are brighter than 7.0 mag. To increase the star density in some regions of the sky, positions and proper motions for additional stars were established on the same system. This catalog contains seven data files, six for different equinoxes (1950, 1955, 1960, 1965, 1970, and 1975) and one for the supplemental stars. The 1950 and 1975 files contain the complete FK4 catalog (1535 stars); the others contain only 52 polar stars. In addition to a header record, the primary catalog contains for each star an identification number; the magnitude (maximum for a variable star); a variability flag, the minimum magnitude for a variable or the magnitude of the secondary for a double star; the HD spectral type and the type for the companion or a second type for a variable star; the position and the change and acceleration of the position; the proper motion and its change with time; the mean epoch of the observations for both right ascension and declination; the standard deviations of the position and proper motion; the numbers of the star in the Boss General Catalog, the N30 catalog, and in the Durchmusterungs; and the parallax. The supplement has a flag to indicate duplicity but no information about variability or the second component. It has no information about the temporal change of the position and proper motion and does not list the N30 and Durchmusterung numbers. It also omits the mean epoch for the observations.
FK4 full catalog for Equinox and Epoch B1950.0 FK4 polar stars for Equinox and Epoch B1955.0 FK4 polar stars for Equinox and Epoch B1960.0 FK4 polar stars for Equinox and Epoch B1965.0 FK4 polar stars for Equinox and Epoch B1970.0 FK4 full catalog for Equinox and Epoch B1975.0 FK4 FK4 star number. --- mpv Photovisual magnitude. mag var If "V", then star is variable. --- mpv2 Fainter mag or 2ndary mag in binary number=1 If a range of magnitudes is given in the book, this contains '-' in 10 and the fainter mag. in 11-12 (F2.1). Similarly, if both components of a double star are catalogued, byte 10 contains '+' and the magnitude of the secondary is in 15-17 (F3.2). Normally 14-17 are blank. mag SpType HD spectral type --- SpType2 Second HD spectral type number=2 If both components of a double star are catalogued, byte 23 contains '+' and 24-26 contain the HD spectral type for the secondary. If the entry is for a single star whose spectrum varies, byte 23 contains '-' and 24-26 contain the second spectral type. Normally 23-26 are blank. --- RAh RA B1950 (hours) h RAm RA B1950 (minutes) min RAs RA B1950 (seconds) s CvarRA Centennial variation (RA) s/ha SvarRA 1/2 the secular variation in RA s/ha2 pmRA Proper motion in RA s/ha d(pmRA) Centennial variation of pmRA s/ha2 EpRA-1900 Epoch (RA) number=3 The first two digits of the year are omitted. (E.g. 1908.22 = 0822) a e_RAs Std dev in RA at mean epoch s e_pmRA Std dev in pm in RA, time sec per trop cy. s/ha DE- Declination sign --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (arc minutes) arcmin DEs Declination B1950 (arc seconds) arcsec CvarDE Centennial variation (Declination) arcsec/ha SvarDE 1/2 the secular variation in Dec arcsec/ha2 pmDE Proper motion in Dec arcsec/ha d(pmDE) Centennial variation of pmDE arcsec/ha2 EpDE-1900 Epoch (Dec) number=3 The first two digits of the year are omitted. (E.g. 1908.22 = 0822) a e_DEs Std dev in Dec at mean epoch arcsec e_pmDE Std dev in pm in Dec, arc sec per trop cy. arcsec/ha GC GC Catalog number (Cat. <I/113>) --- N30 N30 Catalog number (Cat. <I/80>) --- DM Durchmusterung number number=4 Durchmusterung number has form DMSZZNNNNN, where DM='BD', 'CD' or 'CP', and S='+' or '-'. E.g. 'BD+28 4' --- plx Parallax of star. Usually blank arcsec FK4 supplement --- File identifier: 0293 for this file. --- FK4 FK4Sup star number --- GC Boss GC Catalog number (Cat. <I/113>) --- mpv Photovisual magnitude. mag SpType HD spectral type. number=1 Byte 22 is the prefix (blank except for #3505, which is 'c'); 23 is the class; 24 is the subclass; and 25 is the suffix (usually blank, but may be 'p' or 'e'). Two stars have type ' Oe5'. --- double Double star indicator ('2'=double) --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (min) min RAs Right Ascension B1950 (seconds) s pmRA Proper motion in RA, time sec per trop cy s/ha DE- Declination sign --- DEd Declination B1950.0 (degrees) deg DEm Declination B1950.0 (minutes) arcmin DEs Declination B1950.0 (seconds) arcsec pmDE Proper motion in Dec, arcsec per trop cy. arcsec/ha plx Parallax, arc seconds. arcsec fk4_desc.txt Original FK4 catalog description Vincent Kargatis SSDOO/ADF 1997 Jul 24 UNKNOWN UNKNOWN The original machine-readable catalog consisted of seven files broken down by left and right pages for 1950 and 1975, left and right pages for the circumpolar stars, and a file for the supplement. The catalog was supplied to W. M. Owen, Jr. of the Jet Propulsion Laboratory (JPL) in January of 1989. Modifications to the data and format were made at JPL to correct miscellaneous errors, convert old BCD coding to ASCII representation, add Durchmusterung numbers and trigonometric parallaxes, and combine the left and right pages to single files containing one logical record per object in a uniform format. The revised catalog was then returned to the ADC at NASA GSFC, where the descriptive file (also prepared mostly at JPL) was modified. (The logical record length of the Supplement file was changed from 80 bytes to 55 bytes per record at the ADC because bytes 56-80 were blank.) The revised catalog was then archived permanently. * on ADC CD-ROM Volume 1 (October 1991), directory /astrom/fk4 * 24-Jul-1997: Added standardized ReadMe. I_143.xml First, Second and Third Herstmonceux Catalogues for 1950.0 1144 I/144 First, Second and Third Herstmonceux Cats, 1950.0 First, Second and Third Herstmonceux Catalogues for 1950.0 R H Tucker M E Buontempo P Gibbs R H D Swifte R. Greenwich Obs. Bull. No. 189 ??? ??? 1983 1983N84-18125.....T Positional data Proper motions These catalogues contain the results of observations of stars made at the Royal Greenwich Observatory (Herstmonceux) with the Cooke Transit Circle from 1957 October 22 to 1980 November 18.
AGK3R Stars in 1st Hx. Cat. part 2 PZT Stars in 1st Hx. Cat. part 3 Blaauw O,B Stars in 1st Hx. Cat. part 4 Mt. Wilson GCRV Stars in 2nd Hx. Cat. part 2 Variable GCVS Stars in 2nd Hx. Cat. part 3 Robertson's Zodiacal Stars, 3rd Hx. Cat. part 2 Yasuda's NPZT Stars in in 3rd Hx. Cat. part 3 Mt. Wilson GCRV Stars in 3rd Hx. Cat. part 4 cat Catalogue label The following examples demonstrate the format of this field. 1HX502 = First Catalogue, part two 3HX504 = Third Catalogue, part four --- name Star name or number in cat --- Hxnum Herstmonceux number --- Hxc Herstmonceux culmination --- RAh Right Ascension (1950.0) hours h RAm Right Ascension (1950.0) minutes min RAs1 RA (1950.0) seconds: Herstmonceux Observed coordinates for epoch of observation, referred to the equinox of 1950.0, on 1. the Herstmonceux system of star places or 2. the FK4 system of star places The values in these fields are sometimes given greater than 60 (arc)seconds. To find the coordinates in such a case, add one to the (arc)minutes and subtract 60 from the (arc)seconds. The RAm (or DEm) value given applies to whichever RAs (or DEs) value is smaller. This occurs as a result of using one RAm (or DEm) value to describe two different systems and does not indicate errors in the data. s RAs2 RA (1950.0) seconds: FK4 system Observed coordinates for epoch of observation, referred to the equinox of 1950.0, on 1. the Herstmonceux system of star places or 2. the FK4 system of star places The values in these fields are sometimes given greater than 60 (arc)seconds. To find the coordinates in such a case, add one to the (arc)minutes and subtract 60 from the (arc)seconds. The RAm (or DEm) value given applies to whichever RAs (or DEs) value is smaller. This occurs as a result of using one RAm (or DEm) value to describe two different systems and does not indicate errors in the data. s EpRA Epoch of RA: Year-1900 (F6.3) a DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin DEs1 DE (1950.0) arcseconds: Herstmonceux arcsec DEs2 DE (1950.0) arcseconds: FK4 system arcsec EpDE Epoch of Declination: Year-1900 a PlxRA Parallax factor RA AU PlxDE Parallax factor Dec AU o_RAh Number of Observations in R.A. --- o_DEd Number of Observations in Declination --- e_RAs1 Formal Standard Error RA Observed coordinates for epoch of observation, referred to the equinox of 1950.0, on 1. the Herstmonceux system of star places or 2. the FK4 system of star places The values in these fields are sometimes given greater than 60 (arc)seconds. To find the coordinates in such a case, add one to the (arc)minutes and subtract 60 from the (arc)seconds. The RAm (or DEm) value given applies to whichever RAs (or DEs) value is smaller. This occurs as a result of using one RAm (or DEm) value to describe two different systems and does not indicate errors in the data. arcsec e_DEs1 Formal Standard Error Declination arcsec rem Remark D = observation is a duplicate and appears elsewhere within catalogue. --- ADS ADS or IDS ADS number and component or IDS page number and component --- mag Magnitude mag n_mag V = Variable Magnitude --- Sp Spectral type(s) --- r_mag Source catalogue of mag and Sp S = SAO M = Mount Wilson GCRV Z = Robertson's ZC F = FK4 or FK4Sup A = AGK3R data from USNO Washington K = AGK3 V = Various sources --- GC Boss General Catalog number --- HD Henry Draper number --- DMzone Durchmusterung zone --- DM Durchmusterung number --- SAO Smithsonian Astrophys. Obs. Catalog number --- AGKzone AGK zone --- AGK AGK number --- n_AGK Remark on AGK suffix + indicates AGK2 number suffix * indicates Babelsberg number --- Julie Anne Watko SSDOO/ADC 1996 Aug 20 I_144.xml Catalogue of Positions and Proper Motions 1146 I/146 Positions and Proper Motions Catalogue of Positions and Proper Motions S Roeser U Bastian Astron. Astrophys. Suppl. Ser. 74 449 1988 1988A&AS...74..449R Positional data Proper motions PPM North gives J2000 positions and proper motions of 181,731 stars north of -2.5 degrees declination. Its main purpose is to provide a convenient, dense, and accurate net of astrometric reference stars that represents the new IAU (1976) coordinate system on the sky. The mean epoch is near 1931. The average mean errors of the positions and proper motions are 0.27" and 0.43"/cen. On the average six measured positions are available per star; 1064 stars do not have sufficient redundancies to resolve discrepancies. In addition to the positions and proper motions, the PPM (North) contains the BD number, the magnitude, the spectral type, the number of positions included, the mean error of each component of the position and proper motion, the weighted mean epoch in each coordinate, the numbers in the SAO, HD, and AGK3 catalogs, and various standard notes. In addition a number of individual notes are given in the introduction. The PPM North consists of three files: a descriptive document supplied by the authors for more detail regarding the scope, construction, properties, and usage of PPM North; the data file for the PPM North itself; and a version of PPM North in the format of the preliminary PPM North. See author supplied description for more complete information.
Positions and Proper Motions - North PPM Designation of the star Designation of the star in PPM South starting with No. 181732, see chapter 3 of the author's description file. --- DM BD (zones -02 to -22), else CD Designation of the star in the Bonner Durchmusterung (for zones from -02 to -22 degrees) or in the Cordoba Durchmusterung (zones -23 to -89 degrees). --- mag Magnitude See chapter 3 of description file. mag Sp Spectral type --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec pmRA Proper motion in RA, J2000 Proper motion in right ascension fro epoch and equinox J2000.0, on the system of FK5 given in seconds of time per Julian year. s/yr pmDE Proper motion in DE, J2000 arcsec/yr N Number of individual published positions used Number of individual published positions used for the derivation of the position and proper motion given. --- e_RA Mean error of RA Mean error of right ascension at the mean epoch of right ascension, multiplied by the cosine of declination, given in units of #0.01 seconds of arc. 10mas e_DE Mean error of DE Mean error of declination at the mean epoch of declination, given in units of #0.01 seconds of arc. 10mas e_pmRA Mean error of pmRA Mean error of the proper motion in right ascension, multiplied by the cosine of declination, given in units of 0.001 seconds of arc per Julian year. mas/yr e_pmDE Mean error of pmDE mean error of the proper motion in declination given in units of 0.001 seconds of arc per Julian year mas/yr EpRA Weighted mean epoch, RA and pmRA Weighted mean epoch of the measured positions used for the derivation of RA and pmRA, given in years since 1900.0. yr EpDE Weighted mean epoch, DE and pmDE Weighted mean epoch of the measured positions used for the derivation of DE and pmDE, given in years since 1900.0. yr SAO SAO Designation --- HD Henry Draper Designation --- CPD Cape Photographic Durchmusterung Designation --- Flag1 'P' - problem, 'C' - comment P - problem case, preferably not to be used as astrometric reference star. C - a critical comment is given in the List of Critical Comments. Not to be used as astrometric reference star. --- Flag2 'D' - double star D - double star, preferably not to be used as astrometric reference star. --- Flag3 - not used Not used, void for consistency with PPM (north). --- Flag4 'F' - member of FK5 F - member of FK5, mostly bright stars, original FK5 data are given. --- Flag5 'R' - remark, 'V' - V mag (CPC-2) R - a remark is given in the List of Remarks on Individual Stars. V - the magnitude is a photographic V magnitude copied from CPC-2. --- PPM North - in format of old PPM cat The catalog prefix 'PPM' --- PPM Designation of the star --- mag Magnitude mag Sp Spectral type --- Flag1 Problem flag P - problem case, preferably not to be used as astrometric reference star. C - a critical comment is given in the List of Critical Comments. Not to be used as astrometric reference star. --- RA1950 RA equinox and epoch B1950, FK4 rad DE1950 DE equinox and epoch B1950, FK4 rad pmRA1950 Proper motion in RA, B1950, FK4 0.01rad/yr pmDE1950 Proper motion in DE, B1950, FK4 0.01rad/yr RA RA equinox and epoch J2000, FK5 rad DE DE equinox and epoch J2000, FK5 rad pmRA Proper motion in RA, J2000, FK5 0.01rad/yr pmDE Proper motion in DE, J2000, FK5 0.01rad/yr descrip.doc Authors' description Gail L. Schneider NSSDC/ADC 1994 Nov 14 I_146.xml Fifth Fundamental Catalogue (FK5) Part I 1149A I/149A Fifth Fundamental Catalogue Fifth Fundamental Catalogue (FK5) Part I W Fricke H Schwan T Lederle U Bastian R Bien G Burkhardt B du Mont R Hering R Jaehrling H Jahreiss S Roeser H M Schwerdtfeger H G Walter Veroeff. Astron. Rechen-Institut Heidelb. No. 32 ??? ??? 1988 1988VeARI..32....1F I/175 : FK5, Part II (Extension). Argelander, F. W. A. 1859-62, Bonner Sternverzeichniss, erste bis dritte Sektion, Astronomischen Beobachtungen auf der Sternwarte der Koeniglichen Rhein., Friedrich-Wilhelms-Universitaet zu Bonn, Baende 3-5 (Catalog <I/122>) Boss, B. 1937, General Catalogue of 33342 Stars for the Epoch 1950, Carnegie Institution of Washington Pub. 468 (Washington, Carnegie Institution of Washington) (Catalog <I/113>) Cannon, A. J., & Pickering, E. C. 1918-24, The Henry Draper Catalogue, Ann. Astron. Obs. Harvard College, 91-99 (Catalog <III/135>) Corbin, T. E. 1978, in IAU Colloquium 48, Modern Astrometry, ed. F. V. Prochazka & R. H. Tucker (Vienna, University Obs.), p. 505 (Catalog <I/72>) Fricke, W., & Kopff, A. 1963, Fourth Fundamental Katalog (FK4), Veroeff. Astron. Rechen-Inst. Heidelb. No. 10. (Catalog <I/15>) Fricke, W., Schwan, H., & Lederle, T. (in collaboration with Bastian, U., Bien, R., Burkhardt, G., du Mont, B., Hering, R., Jaehrling, R., Jahreiss, H., Roeser, S., Schwerdtfeger, H. M., & Walter, H. G.) 1988, Fifth Fundamental Catalogue (FK5), Part I. The Basic Fundamental Stars, Veroeff. Astron. Rechen-Institut Heidelb. No. 32 (Catalog <I/149>) Gill, D., & Kapteyn, J. C. 1895-1900, Cape Photographic Durchmusterung, Ann. Cape Obs., 3 (1895, Part I: zones -18 deg. to -37 deg.); 4 (1897, Part II: zones -38 deg. to -52 deg.); 5 (1900, Part III: zones -53 deg. to -89 deg.) (Catalog <I/108>) Kuestner, F. 1903, Bonner Durchmusterung des Noerdlichen Himmels, zweite berichtigte Auflage, Bonn Universitaets Sternwarte (Bonn, A. Marcus und E. Weber's Verlag) (Catalog <I/122>) Lieske, J. H. 1979, Astron. & Astroph., 73, 282 (=1979A&A....73..282L) Nicolet, B. 1975, Catalogue of Measurements in the Cape UBV Photometry on Magnetic Tape, Astron. & Astroph. Supp., 22, 239 (Catalog <II/27>) Nicolet, B. 1978, Catalogue of Homogeneous Data in the UBV Photoelectric Photometric System, Astron. & Astroph. Supp., 34, 1 (=1978A&AS...34....1N) Schoenfeld, E. 1886, Bonner Sternverzeichniss, vierte Sektion, Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rheinischen Friedrich-Wilhelms-Universitaet zu Bonn, 8, Part IV (Bonn, Adolph Marcus Verlag) (Catalog <I/119>) Scott, F. P., & Smith, C. A., Jr. 1971, Comparison of the SAO and AGK3R Star Catalogues, in Conference on Photographic Astrometric Techniques, ed. H. K. Eichhorn, NASA CR-1825 Smith, C. A., Corbin, T. E., Hughes, J. A., Jackson, E. S., Krutskaya, E. V., Polozhentsev, A. D., Polozhentsev, D. D., Yagudin, L. I., & Zverev, M. S. 1990, in IAU Symposium No. 141, Inertial Coordinate System on the Sky, ed. J. H. Lieske & V. K. Abalakin (Dordrecht, Reidel), p. 457 (Catalog <I/138>) Thome, J. M. 1892-1932, Cordoba Durchmusterung, Resultados del Observatorio Nacional Argentino, 16 (1892, Part I: -22 deg. to -32 deg.); 17 (1894, Part II: -32 deg. to -42 deg.); 18 (1900, Part III: -42 deg. to -52 deg.); 21 (Part I) (1914, Part IV, -52 deg. to -62 deg.); 21 (Part II) (1932, Part V: -62 deg. to -90 deg.) (Catalog <I/114>) Proper motions Positional data The Basic Fifth Fundamental Catalogue (FK5) Part I provides improved mean positions and proper motions for the 1535 classical fundamental stars that had been included in the FK3 and FK4 catalogs. The machine version of the catalog contains the positions and proper motions of the Basic FK5 stars for the epochs and equinoxes J2000.0 and B1950.0, the mean epochs of individual observed right ascensions and declinations used to determine the final positions, the mean errors of the final positions and proper motions for the reported epochs, and ancillary data such as magnitudes, spectral types, parallaxes, radial velocities, and cross identifications to other catalog designations.
The Basic FK5 is the successor to the FK4 (Fricke & Kopff 1963) and contains the 1535 classical fundamental stars used to define the latter system. It represents a revision of the FK4 and results from the determination of systematic and individual corrections to the mean positions and proper motions of the FK4, the elimination of the error in the FK4 equinox, and the introduction of the IAU (1976) system of astronomical constants. About 300 catalogs providing star positions obtained from throughout the world are included in the FK5. This document should be used only to supplement the information contained in the source reference. The latter should be consulted for more detailed information regarding the motivation for construction of the FK5, the determination of its equator and equinox, the expressions for general precession, a discussion of the FK5 system, systematic differences between the FK4 and FK5, the transformation of observational catalogs to the FK5 system and to the reference system J2000.0, and more thorough descriptions of the data contained in the FK5 catalog.
The FK5 catalog FK5 FK5 number These numbers have remained the same from the FK3 and FK4 (Catalog <I/15>). The user should note that the file is ordered by FK5 number, which means that the stars are arranged neither by right ascension nor by declination. --- RAh Right ascension, hours, Equinox=J2000, Epoch=J2000 h RAm Right ascension minutes (J2000.0) min RAs Right ascension seconds (J2000.0) The terms of elliptic aberration have been eliminated from the mean positions. The B1950.0 data have been computed from the J2000.0 data using a procedure described in the source reference (Fricke et al. 1988) based on the IAU (1976) system of astronomical constants (see also Lieske 1979). s pmRA Proper motion in RA (J2000.0) s/ha DE- Sign of declination (Dec) (J2000.0) --- DEd Declination degrees (J2000.0) deg DEm Declination arcminutes (J2000.0) arcmin DEs Declination arcseconds (J2000.0) arcsec pmDE Proper motion in DE (J2000.0) arcsec/ha RAh1950 Right ascension, hours Equinox=B1950, Epoch=B1950 h RAm1950 Right ascension minutes (B1950.0) min RAs1950 Right ascension seconds (B1950.0) s pmRA1950 Proper motion in RA (B1950.0) s/ha DE-1950 Sign of declination (B1950.0) --- DEd1950 Declination degrees (B1950.0) deg DEm1950 Declination arcminutes (B1950.0) arcmin DEs1950 Declination arcseconds (B1950.0) arcsec pmDE1950 Proper motion in DE (B1950.0) arcsec/ha EpRA-1900 Mean Epoch of observed RA Mean epoch (-1900.0) of the individual observed right ascensions and declinations. a e_RAs Mean error in RA The mean errors of the positions at the mean epoch and of the corresponding proper-motion components, as obtained from the solution of the normal equations within the derivations of individual positions and proper motions. (These mean errors do not include those of the FK5 system and of the equinox and equator.) ms e_pmRA Mean error in pmRA ms/ha EpDE-1900 Mean Epoch of observed DE a e_DEs Mean error in Declination carcsec e_pmDE Mean error in pmDE carcsec/ha Vmag V magnitude Photoelectric magnitudes on the UBV system, as taken from the catalogs of Nicolet (1975, 1978). Variability is indicated by a flag in byte 129. For physical double stars, the magnitudes of the brighter components are given (both are given in the published catalog). mag n_Vmag Magnitude flag Where magnitude ranges are given in the published catalog, the brighter magnitude is given and byte 129 contains an upper case "V". A lower case "v" is present if there is variability and that letter is present in the published catalog (amplitude exceeds 0.3mag). A "D" code indicates that the magnitudes of two close components are given as a footnote in the published catalog. Only the first of the two is contained in the magnitude field of the machine-readable catalog. --- SpType Spectral type(s) A one-dimensional spectral type taken from the FK4 catalog. These types are from the Henry Draper Catalogue (Cannon & Pickering 1918-24). For binary and multiple systems where spectral types are known for more than one component, a second spectral type may be given following a plus sign. --- plx Parallax Trigonometric parallax if known (blank otherwise). These data are taken from a preliminary version of the new Yale parallax catalog (van Altena, Lee, & Hoffleit, in preparation). Negative parallaxes present in the Yale catalog have been omitted here because they are of no use in computing apparent places from the mean positions. arcsec RV Radial velocity Radial Velocity if known (blank otherwise) km/s AGK3R AGK3R number (Catalog <I/72>) --- SRS SRS number (Catalog <I/138>) --- HD HD number (Catalog <III/135>) --- DM DM identifier the prefixes are BD: Bonner Durchmusterung (Argelander 1859-62, Kuestner 1903) SD: Southern Durchmusterung (Schoenfeld 1886) CD: Cordoba Durchmusterung (Thome 1892-1932) CP: Cape Photographic Durchmusterung (Gill & Kapteyn 1895-1900) --- GC GC number (Catalog <I/113>) --- Nancy G. Roman ADC/SSDOO rev. Francois Ochsenbein CDS 1995 Jun 13 Dr. H. Schwan kindly supplied the original and revised versions of the on magnetic tape and colleagues at the Astronomisches Rechen-Institut generously reviewed a draft copy of the original documentation prior to its final release for distribution with machine-readable copies of the catalog, and Dr. Schwan returned comments and corrections. Appreciation is expressed to Dr. William M. Owen Jr. of JPL for supplying the machine-readable FK4, DM cross index that was used to insert DM numbers into the original version of the FK5 catalog. UNKNOWN UNKNOWN The following format changes were made by W. H. Warren Jr. (with Dr. Schwan's concurrence): The DM identifiers, which were single-digit numerical codes, were changed to the literal codes. Plus signs were added to the trigonometric-parallax data, even though no negative parallaxes are included in the catalog, to indicate that negative parallaxes are possible. Multiple blanks between data fields were removed, as were blanks beyond the end of each record, to decrease the logical record length from 220 bytes to 190 bytes. I_149A.xml The Catalogue of Proper Motions for High Luminosity Stars 1150 I/150 Proper Motions for High Luminosity Stars The Catalogue of Proper Motions for High Luminosity Stars A M Valitova D K Karimova E D Pavlovskaya Tr. Gos. Astron. Inst. Sternberg ??? ??? 1990 1990 Proper motions Stars, luminous Meridian circle observations of high luminosity stars were used to supplement previous positions to derive improved proper motions. The proper motions and positions are derived for J2000.0 and for the epoch of observation but the systematic correction: FK5-FK4 and the correction to FK5 for each star were ignored. V magnitudes and MK spectral types are taken from published catalogs.
The stars selected for observation were taken from lists provided by Parenago and by Blaauw supplemented by lists compiled at the Sternberg Institute. The proper motions were taken from papers by Karimova, Pavlovskaya, and Toropova (1974) and Karimova and Pavlovskaya (1981) supplemented by new positional catalogs published after these papers were written. For GC stars, the number of catalogs used to refine the GC motions is given; for other stars, the complete number of catalogs used is listed. The method described in the GC (Boss, 1937) is employed with weights of additional catalogs taken from Karimova and Pavlovskaya (1971), from the published internal errors, or from the table from Karimova and Pavlovskaya (1971). To convert from B1950.0 to J2000.0, the standard matrix method from the Astronomical Almanac for 1989 was used.
catalog ID Sequential number --- HD Number in HD catalogue If star is absent in HD catalogue, then its BD number is given. --- Sp MK spectral and luminosity class --- V V magnitude mag RAh Right Ascension (J2000.0) hours Right Ascension and Declination for J2000.0 and for epoch of J2000.0 and for epoch of observations in FK5 system. h RAm Right Ascension (J2000.0) minutes min RAs Right Ascension (J2000.0) seconds s DE- Declination (J2000.0) sign --- DEd Declination (J2000.0) degrees deg DEm Declination (J2000.0) arcminutes arcmin DEs Declination (J2000.0) arcseconds arcsec pmRA Proper motion in RA equinox J2000.0 (J years) s/a e_pmRA Error of pmRA (J years) s/a EpRA Epoch of observations for RA (B years) a catRA Number of catalogues RA Number of catalogues that were used to define more precisely proper motions in Right Ascension or Declination. --- pmDE Proper motion in DE equinox J2000.0 (J years) arcsec/a e_pmDE Error of pmDE arcsec/a EpDE Epoch of observations for DE (B years) a catDE Number of catalogues DE --- Julie Anne Watko SSDOO/ADC 1996 May 20 I_150.xml Precise Radio Source Positions Determined by Mark III VLBI: Observations from 1979 to 1988 and a Tie to the FK5 1151 I/151 Precise Radio Source Positions from Mark III VLBI Precise Radio Source Positions Determined by Mark III VLBI: Observations from 1979 to 1988 and a Tie to the FK5 C Ma D B Shaffer C de Vegt K J Johnston J L Russell AJ 99 1284 1990 1990AJ.....99.1284M Radio sources Positional data VLBI This catalog contains observations from 600 Mark III VLBI experiments from conducted between 1979 to 1988. These experiments resulted in 237681 acceptable pairs of group delay and phase delay rate observations. These have been used to derive positions of 182 extra-galactic radio sources with typical formal standard errors less than 1 mas. The right ascension zero point of this reference frame has been aligned with the FK5 by using the optical positions of 28 extragalactic radio sources whose positions are on the FK5 system. Also included are the Mark III VLBI stations and a summary of the analysis configuration.
Source positions (J2000) from GLB353 solution IAU IAU name of radio source --- Other Other name of radio source --- RAh right ascension (hours) (J2000) The positions are relative to the J2000.0 coordinate system as defined by the conventional models on the reference date 1980 October 17.The right ascension zero point is defined by minimizing the adjustment of the right ascensions, scaled by cos DE, of the 28 sources with FK5 positions from the values given in table4 h RAm right ascension (minutes) (J2000) min RAs right ascension (seconds) (J2000) s e_RAs standard error of RA (seconds) (J2000) The standard errors given are the formal 1e errors from the GLB353 solution scaled by the square root of the reduced chi-square of the solution. See text. s DE- declination sign (J2000) --- DEd declination (degrees) (J2000) deg DEm declination (minutes) (J2000) arcmin DEs declination (seconds) (J2000) arcsec e_DEs standard error of DE (seconds) arcsec CORR RA-DE correlation --- EPOCH Mean Julian epoch a NEXP number of experiments --- NOBS number of observations --- FK5 optical positions of 28 extragalactic IAU IAU name of radio source --- Other Other name of radio source --- RAh right ascension (hours) (J2000) h RAm right ascension (minutes) (J2000) min RAs right ascension (seconds) (J2000) s DE- declination sign (J2000) --- DEd declination (degrees) (J2000) deg DEm declination (minutes) (J2000) arcmin DEs declination (seconds) (J2000) arcsec TYPE radio source types QSO=quasar, BLO=BL Lac object, GAL=galaxy -------------------------------------------------------------------------------- Table 1: Mark III VLBI stations ------------------------------------------------------ ALGOPARK Algonquin Park, Ontario, Canada CHLBOLTN Chilbolton, U.K. EFLSBERG Effelsberg, F.R.G. GILCREEK Fairbanks, Alaska GOLDVENU Fort Irwin, California HARTRAO Johannesburg, South Africa HATCREEK Hat Creek, California HAYSTACK Westford, Massachusetts HRAS 085 Fort Davis, Texas KASHIMA Kashima, Japan KAUAI Kauai, Hawaii KWAJAL26 Kwajalein Atoll, Marshall Islands MARPOINT Maryland Point, Maryland MEDICINA Medicina, Italy MOJAVE12 Fort Irwin, California NRAO 140 Green Bank, West Virginia ONSALA60 Onsala, Sweden OVRO 130 Big Pine, California PENTICTN Penticton, British Columbia, Canada(*) PLATTVIL Platteville, Colorado(*) RICHMOND Richmond, Florida ROBLED32 Madrid, Spain VNDNBERG Vandenburg Air Force Base, California WESTFORD Westford, Massachusetts WETTZELL Wettzell, F.R.G. YELLOWKN Yellowknife, Northwest Territories, Canada(*) ------------------------------------------------------ (*) Mobile VLBI site. Table 2: Summary of analysis configuration ------------------------------------------------------------------ Models: Solar system - PEP planetary ephemeris Precession and sidereal time - J2000.0 Nutation - IAU 1980 (see also parameters) Solar relativistic deflection of light Solid earth tides Calibrations: Troposphere - CfA 2.2 using meteorological data Chao if no meteorological data Ionosphere - simultaneous S/X observations Length of timing signal/phase cal cable Parameters: Global - Source positions (adjusted) Arc - Site positions Nutation offsets in longitude and obliquity Polynomial and sinusoidal clocks Zenith atmosphere delays Constrained atmosphere rates Reference Date: 1980 October 17 Data: Mark III group delays and phase delay rates Observations: 237681 --- James E. Gass SSDOO/ADC 1998 Feb 13 I_151.xml Lick Jupiter-Voyager Reference Star Catalogue 1152 I/152 Lick Jupiter-Voyager Reference Star Catalogue Lick Jupiter-Voyager Reference Star Catalogue A R Klemola L Morabito H Taraji Lick Obs., U. California, Santa Cruz. ??? ??? 1978 1978 I/125 : Combined Lick-Voyager Reference Star Catalogue (Dunham 1986) I/153 : Lick Saturn-Voyager Reference Star Catalogue (Klemola+, 1979) Dieckvoss W., Kox H., Guenther A., and Brosterhus E. 1975, AGK3. Star catalogue of positions and proper motions north of -2.5 deg. declination, derived from plates taken at Bergedorf and Bonn in the years 1928-1932 and 1956-1963., Hamburger Sternwarte, Hamburg-Bergedorf. (see catalogue <I/69>) Klemola A. R. (Lick Obs.), Morabito L., and Taraji H. (Jet Propulsion Lab.) 1978, Lick Jupiter-Voyager Reference Star Catalogue., Lick Observatory, University of California, Santa Cruz. Klemola A. R. (Lick Obs.), Morabito L., and Taraji H. (Jet Propulsion Lab.) 1979, Lick Jupiter-Voyager Reference Star Catalogue., Lick Observatory, University of California, Santa Cruz. Lopez C. E. 1988, Pub. Astron. Soc. Pacific. 100, 1273. (1988PASP..100.1273L) Positional data Zodiacal regions The catalog was prepared for purposes of determining up-to-date, reasonably accurate equatorial coordinates for reference stars in a band of sky against which cameras of the Voyager spacecraft were aligned for observations of Jovian satellites during the Jupiter flyby. The catalog contains accurate equatorial coordinates for equinox 1950.0, epoch 1978.27, photographic and visual magnitudes, AGK3 identifications and proper motions for 4983 stars. All of the reference stars are in the range 6h00m to 8h04m in right ascension (1950), declination zones +16 to +23 degrees, and 8h31m to 8h57m, zones +08 to +14 degrees. Mean errors of the positions are about 0.4 second of arc.
The Lick Jupiter-Voyager Reference Star Catalogue. Klemola et al. (1978) was prepared for purposes of determining up-to-date, reasonably accurate, equatorial coordinates for reference stars in a band of sky against which cameras of the Voyager spacecraft were aligned for observations of Jovian satellites during the Jupiter flyby. The requirements were a surface density of three to four reference stars per observation frame of 24 sq. arcmin. of the cameras - somewhat greater than that provided by the AGK3 catalog (Dieckvoss et al. 1975) - and a positional accuracy approximately 0.5. Visual magnitudes were also required. The completed catalog contains 4983 stars in the right ascension ranges 6h00m to 8h04m, declination zones +16 deg. to +23 deg., and 8h31m to 8h57m, declination zones +08 deg. to +14 deg.. Mean errors of the positions, as derived from least squares solutions against the AGK3 reference stars, are about 0.4"; however, individual residuals are fairly numerous in the range 0.6" to 0.8" with some in the range 1.0" to 1.3" The accidental error of one measurement, as deduced from a tabular histogram given in the original catalog publication (referenced below), is about 0.11". Apparent photographic and visual magnitudes were derived from iris photometer measurements, m(v). being approximated from a derived color-index relation using the AGK3 reference stars. The resulting magnitudes appear to have mean errors of at least 0.2 mag while very blue and very red stars (C.I..le.0 mag, and C.I..ge.1.5, respectively) are less certain. The magnitudes are considered to be only approximate (residuals of approximately 0.5 mag are fairly common). For additional information concerning the observations and reductions, the original publication (available from A. R. Klemola) should be consulted. A copy of this document should be transmitted to any recipient of the machine-readable catalog.
The catalogue Seq Running star number A running star number denoting the order in which stars were selected for measurement on each plate. --- plate Plate number --- RAh Right ascension (1950.0), Epoch=1978.27 Equatorial coordinates given for Equinox 1950, Epoch 1978.27 h RAm Right ascension (1950.0) minutes min RAs Right ascension (1950.0) seconds s DE- Sign of declination zone --- DEd Declination (1950.0), Epoch=1978.27 deg DEm Declination (1950.0) arcminutes arcmin DEs Declination (1950.0) arcseconds arcsec Pmag Photographic magnitude Apparent photographic magnitude, m(pg), as determined from iris photometry. mag Vmag Visual magnitude Apparent visual magnitude, m(v), approximated from m(pg) and a derived color-index relation using the AGK3 reference stars. mag AGK3 AGK3 (catalog <I/69>) designation --- pmRA Centennial Proper motion in RA The centennial proper motions (pmRA, pmDE). These data are taken from the AGK3 catalog. The proper motions in right ascension are given as the great circle measures (pmRA*cos(declination)). 10mas/a pmDE Centennial Proper motion in RA 10mas/a Aug-31-1995 revised J.A. Watko SSDOO/ADC 1996 Apr 26 Appreciation is expressed to A. R. Klemola for providing the magnetic tape of the catalog and for reviewing the modifications made to the data. Dr. Klemola also kindly reviewed a draft copy of this document before its completion and printing. The work of W. M. (Bill) Owen, Jr., in correcting and updating the earlier version of the catalog, is gratefully acknowledged, as are his comments on the statistical accuracy of the positions and the revised documentation. I_152.xml Lick Saturn-Voyager Reference Star Catalogue 1153 I/153 Lick Saturn-Voyager Reference Star Catalogue Lick Saturn-Voyager Reference Star Catalogue A R Klemola H Taraji A Ocampo Lick Observatory, University of California, Santa Cruz ??? ??? 1979 1979 I/152 : Lick Jupiter-Voyager Reference Star Catalogue (Klemola+ 1978) I/125 : Combined Lick-Voyager Reference Star Catalogue (Dunham 1986) Blanco, V. M., Demers, S., Douglass, G. G., and FitzGerald, M. P. 1968, Publ. U. S. Naval Obs., 2nd Ser., 21. Dieckvoss, W., Kox, H., Guenther, A., and Brosterhus, E. 1975, AGK3. Star catalogue of positions and proper motions north of -2.5 deg. declination, derived from plates taken at Bergedorf and Bonn in the years 1928-1932 and 1956-1963, Hamburger Sternwarte, Hamburg-Bergedorf. Hoeg, E. and von der Heide, J. 1976, Perth 70, A Catalogue of Positions of 24900 Stars, Abh. der Hamburger Sternwarte, Band IX. (Catalog <I/62>) Klemola, A. R. (Lick Obs.), Taraji, H., and Ocampo, A. (Jet Propulsion Lab.) 1979, Lick Saturn-Voyager Reference Star Catalogue, Lick Observatory, University of California, Santa Cruz. Smithsonian Astrophysical Observatory Staff 1966, Star Catalog. Positions and Proper Motions of 258,997 Stars for the Epoch and Equinox of 1950.0, Publ. of the Smithsonian Institution of Washington, DC No. 4652 (Washington: Smithsonian Institution). (See cat. <I/131>) Positional data Regional catalog The Lick Saturn-Voyager Reference Star Catalogue contains accurate equatorial coordinates for 4551 stars in a band of sky against which cameras of the Voyager spacecraft were pointed for observations in the region of Saturn during the flyby. All of the reference stars are in the range 12h 40min to 14h 12min in right ascension (1950) and +02deg. to -09deg. in declination. Mean errors of the positions are about 0.25".
The Lick Saturn-Voyager Reference Star Catalogue was prepared for purposes of determining up-to-date, reasonably accurate, equatorial coordinates for reference stars in a band of sky against which cameras of the Voyager spacecraft were aligned for observations in the region of Saturn during the flyby. The requirements were a surface density of about three reference stars per observation frame of 24 sq.arcmin of the cameras - somewhat greater that the SAO (Smithsonian Astrophsyical Observatory Staff 1966) and the AGK3 (Dieckvoss et al. 1975) densities - and a positional accuracy +/- 0.5". Visual magnitudes were also required. The completed catalog contains 4551 stars in the right ascension range 12h 40min to 14h 12min, declination zones +02deg. to -09deg. Mean errors of the positions, as derived from least squares solutions against the Perth 70 Catalogue (Hoeg and von der Heide 1976), are about 0.25"; however, individual residuals for some bright and excessively faint stars are as high as 0.5" to 1.0". The accidental error of one measurement, as deduced from a tabular histogram given in the original catalog publication (referenced below), is about 0.09". Apparent photographic and visual magnitudes were derived from iris photometer measurements, visual magnitude being approximated from a derived color-index relation using UBV stars selected from the USNO photoelectric catalog (Blanco et al. 1968) and extended with Perth 70 stars. The resulting magnitudes appear to have mean errors of at least 0.2mag - 0.3mag for the brighter stars (visual magnitude < 10mag) and uncertainties can be as much as 0.5mag for the fainter stars. The magnitudes are considered to be only approximate, especially on the faint end, because of a lack of photoelectric standards there. For additional information concerning the observations and reductions, the original publication (available from A. R. Klemola) should be consulted.
*The catalog num Running star number --- pl_num Plate number --- RAh Right ascension, hours (Eq=1950, Ep=1978.92) Equinox=1950, Epoch=1978.92. h RAm Right ascension, minutes (1950) min RAs Right ascension, seconds (1950) s DE- Sign of declination zone --- DEd Declination degrees (1950) deg DEm Declination arcminutes (1950) arcmin DEs Declination arcseconds (1950) arcsec Pmag Photographic magnitude (1950) Determined from iris photometry. mag Vmag Visual magnitude Apparent visual magnitude, m(v), approximated from visual magnitude and a derived color-index relation using UBV stars selected from the USNO photoelectric catalog of Blanco et al. (1968) and extended with Perth 70 stars. mag Name Alternate identification AGK3 or SAO identification number. For AGK3 numbers, bytes 39-41 contain the zone and bytes 42-46 the number. SAO numbers are contained in bytes 41-46. --- pmRA Proper motion in right ascension These data are taken from the AGK3 or SAO catalogs. The proper motions in right ascension are given as the great circle measures. 10mas/a pmDE Proper motion in declination 10mas/a Nancy G. Roman ADC/SSDOO 1995 May 02 Appreciation is expressed to A. R. Klemola for providing the magnetic tape of the catalog and for reviewing the modifications made to the data. Dr. Klemola also kindly reviewed a draft copy of this document before its completion and printing. The work of W. M. (Bill) Owen, Jr., in correcting and updating the earlier version of the catalog, is gratefully acknowledged, as are his comments on the statistical accuracy of the positions and the revised documentation. This document was written by Wayne H. Warren Jr. and was translated from a Script version to the current standard ASCII form. UNKNOWN UNKNOWN A magnetic tape containing the catalog, in binary format, was received from Dr. A. R. Klemola in November 1981. The data were converted to character-coded form and written to a direct access storage device for editing. The following modifications were made to the data in order to effect a more uniform format and to standardize the data representation: Plus signs were added to all positive declination zones. Missing data were converted from zeros to blanks. Since there are valid zero proper-motion data in the catalog, the source reference had to be scanned visually to locate all these values so that they could be converted back to zeros again. In the original machine-readable file, there was no way to tell between zero proper motions and missing values. All AGK3 numbers were converted to the representation +/-XX XXXX (SAO numbers were not modified). The catalog was sorted by increasing right ascension (the stars were originally in some kind of plate or measurements order). A copy of the catalog, originally archived and documented at the ADC in 1982, was sent to W. M. Owen, Jr. of the NASA Jet Propulsion Laboratory, in January 1990. Mr. Owen, having collaborated with Dr. Klemola in the preparation of the Lick Reference catalogs for the Uranus and Neptune encounters, reviewed the catalog and made the following modifications to the file: AGK3 designations and proper motions were added for 17 stars not previously identified as AGK3 stars. SAO numbers and proper motions were added for eight stars not previously identified as SAO stars. Four stars appeared in the catalog twice. Their positions and magnitudes were averaged and the duplicate entries deleted. Stars 575/8718 and 219/8718 were incorrectly identified as SAO stars; their identification and proper-motion fields were blanked out. Three AGK3 and six SAO designations were erroneous and were corrected. (The proper motions were found to be correct for these entries, however.) I_153.xml Astrographic Catalogue, Zones -02 to +31 degrees Right Ascension and Declination Files 1154 I/154 Astrographic Catalogue, Zones -02 to +31 degrees Astrographic Catalogue, Zones -02 to +31 degrees Right Ascension and Declination Files S Roeser Astronomisches Rechen-Institut, Heidelberg, ??? ??? 1990 1990 Astrometric data The "Astrographic Catalogue" (or "Carte de Ciel") is a catalogue of star positions and magnitudes, determined on the photographic plates taken by the normal astrographs which are installed in observatories of various latitudes, as a world-wide astronomical project (see Eichhorn, 1974, p279). The catalogue is divided into 22 declination zones, each of which is assigned to each observatory, e.g., a zone from +18 to +24 degrees is to Paris observatory. A part of this catalogue, i.e., zones from -02 to +31 degrees, was once recompiled by using AGK2/3 catalogue as the reference (Lacroute 1981), and is already archived in CDS as catalogues I/21 and 22. The present catalogue gives the result of recalculation of the same zones, by using AGK3 catalogue (printed Hamburg version) as the reference. Note that since the content of stars per plate has not been checked, there may be some entries missing. The participated observatories and the archived files are as follows: ------------------------------------------------------ declination zone observatory file ------------------------------------------------------ -02 to +04 Algiers f1 +05 to +10 Toulouse f2 +11 to +17 Bordeaux f3 +18 to +24 Paris f4 +25 to +31 Oxford I f5 ------------------------------------------------------ Note that +11 degree zone is also observed by Toulouse, and the results are included in the file f2 . References Eichhorn, H. (1974): Astrometry of Star Positions, Frederick Unger Publ. Co., New York. Lacroute, P. (1981): Bull. Inform. CDS, Vol.21, p2.
Algiers zone (-02,-01,+00,+01,+02,+03,+04) Toulouse zone (+05 to +10 and +11 degree) Bordeaux zone (+11 to +17 degree) Paris zone (+18 to +24 degree) ZONE plate identifier Declination zone or the declination of the center of each astrographic plate. deg PLATE plate identifier Running number of plate in the zone. --- HYPH hyphen number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. --- id running number of star on the plate number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. --- RAh right ascension (hours) [B1950] number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. h RAm right ascension (minutes) number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. min RAs right ascension (seconds) number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. s DE- declination sign number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. --- DEd declination (degrees) [B1950] number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. deg DEm declination (minutes) number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. arcmin DEs declination (seconds) number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. arcsec Epoch plate epoch number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. a mag photographic magnitude number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. mag AGKNO AGK3 number AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. --- SUFFIX blank Will be used for the suffix to the AGK3 number but not yet used. number= Declination zone or the declination of the center of each astrographic plate. number= Running number of plate in the zone. number= AGK3 number if AGK3 star was identified in Strasbourg; otherwise blank. Note, a survey of 100000 records in f1 found no AGK3 numbers. col. 48-50 may be, e.g., ' -1', '-01', '+01', '&01', ' +1', ' -', etc. Note, a survey of 100000 records in f1 found no AGK3 numbers. number= Will be used for the suffix to the AGK3 number but not yet used. --- Oxford I zone (+25 to +31 degree) ZONE plate identifier See notes for f1, f2, f3, and f4. deg PLATE plate identifier --- HYPH hyphen number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. --- id running number of star in the zone This number is so counted as to be unique in the zone. number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. --- RAh right ascension (hours) [B1950] number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. h RAm right ascension (minutes) number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. min RAs right ascension (seconds) number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. s DE- declination sign number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. --- DEd declination (degrees) [B1950] number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. deg DEm declination (minutes) number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. arcmin DEs declination (seconds) number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. arcsec EPOCH plate epoch number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. a mag photographic magnitude number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. mag AGKNO AGK3 number, if AGK3 star was identified in number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. --- SUFFIX blank number= See notes for f1, f2, f3, and f4. number= This number is so counted as to be unique in the zone. --- Nancy Grace Roman ADC/SSDOO 1996 May 09 This ReadMe is a standardization of the Intro file prepared by Koichi Nakajima [CDS] on 1-Sept-1993. I_154.xml The U.S. Naval Observatory Zodiacal Zone Catalog 1157 I/157 U.S. Naval Observatory Zodiacal Zone Catalog The U.S. Naval Observatory Zodiacal Zone Catalog G G Douglass R S Harrington AJ 100 1712 1990 1990AJ....100.1712D Positional data Proper motions The catalog provides positions and proper motions at equinox and epoch J2000.0, on the FK5 system, for stars in the magnitude range 4-10, lying within 16 degrees of the ecliptic and north of declination -30 degrees. In order that references to earlier catalogs can be made, the B1950.0 positions and proper motions are given in both the FK5 and the FK4 systems. Other useful information, such as visual magnitudes and spectral types, is also provided. Stellar identification is strictly by Durchmusterung number, and the catalog is ordered by J2000.0 right ascension. It is important to understand that the present catalog does not cover the entire zodiacal zone, since stars south of zone -29 degrees could not be observed from the Washington site. These will be observed from the USNO Black Birch station in New Zealand commencing in 1991.
Catalog Data DM_cat Durchmusterung Catalog BD Bonner Durchmusterung CD Cordoba Durchmusterung --- DM Durchmusterung Number --- mag Visual Magnitude mag RAh Right Ascension (J2000) hours h RAm Right Ascension (J2000) minutes min RAs Right Ascension (J2000) seconds s pmRA Proper Motion in RA(2000), seconds/Julian yr s/a DE- Declination (J2000) sign --- DEd Declination (J2000) degrees deg DEm Declination (J2000) arcminutes arcmin DEs Declination (J2000) arcseconds arcsec pmDE Proper Motion in Dec(2000), arcsec/Julian yr arcsec/a Sp Spectral Type --- Ep Position Epoch - 1900 a RA20 Right Ascension (J2000) hours h DE20 Declination (J2000) degrees deg RA50 Right Ascension (B1950) hours h DE50 Declination (B1950) degrees deg pmRA50 Proper Motion in RA (B1950) s/a pmDE50 Proper Motion in Dec (B1950) arcsec/a Julie Anne Watko SSDOO/ADC 1996 Feb 21 I_157.xml AGK3R 1161 I/161 AGK3R AGK3R C A Smith Jr. unpublished, ??? ??? 1990 1990 Positional data Proper motions A catalog of positions of reference stars distributed uniformly on the celestial sphere north of declination -5 deg. contains meridian observations of 21,499 stars with a mean epoch 1958.5. This catalog was compiled from more than 300,000 observations made with 11 northern meridian circles during the period 1956 to 1963. The observations are on the FK4 system.
There is a need for reference catalogs with good modern positions. Recently, positions were redetermined for Northern Hemisphere reference stars to form the AGK3R catalog that was used to determine the plate constants for the AGK3 Photographic Catalog (Dieckvoss 1975). The AGK3R catalog contains 21,499 stars evenly distributed on the surface of the celestial sphere from -5 deg. to +90 deg. The observations were made with 11 northern meridian circles during the period 1956 to 1963. Stars were selected from two lists: one selected at the U. S. Naval Observatory and the other at the Pulkovo Observatory and the Sternberg Institute. The participating observatories were Bergedorf, Bordeaux, Greenwich, Heidelberg, Nicolaev, Ottawa, Paris, Pulkovo, Strasbourg, and the U. S. Naval Observatory (Smith, 1980). Both the seven-inch and the six-inch transit circles were employed at the U. S. Naval Observatory. All observations were reduced on a nightly basis by the observers to the FK3R system and, later to the FK4 either by the observer himself or at the U.S. Naval Observatory.
Data ID AGK3R number Four stars appeared twice in the original AGK3R observing list under different serial numbers. The data from the duplicate stars have been combined and the stars renumbered (AGK3R numbers). The duplicate stars removed and the number assigned in the new numbering system are as follows: Current AGK3R Number Duplicate AGK3R Numbers in Observing List ------------------------------------------------------- 1930C 1931, 1932 2405C 2407, 2408 2951C 2954, 2955 3633C 3637, 3638 --- lcode List code S = U. S. Naval Observatory List Z = Pulkovo Observatory and Sternberg Institute List C = Both lists --- ob_id AGK3R number in the observing list --- DMz BD Zone --- DMno BD number The only star without a DM number is 1135Z. It was formerly listed as BD-01 deg.170A but has no connection with BD-01 deg.170. --- mag Magnitude mag Sp Spectral type An & in byte 23 indicates that the spectrum is composite. The types for these stars are as follows: AGK3R Number Spectral Types --------------------------------------- 4536C A + G 4996S F8 + A0 5217S A0 + G0 5739S F0 + A2 6063S F5 + A5 6123S F5 + A3 6324S F5 + A 6754S A2 + G 7251S F2 + A2 8698S F2 + A2 10048S F5 + A5 11154S F5 + A3 12871S F5 + A0 13650S A2 + G 16982S A0 + G 17619S K0 + A0 17641S F5 + B8p 18095S G0 + A 18453S F5 + A3 18727S K0 + A2 19812S G5 20257S A3 + G --------------------------------------- --- RAh Right ascension, hours (1950) h RAm Right ascension, minutes (1950) min RAs Right ascension, seconds (1950) s e_RAs Mean error of RA reduced to equator s o_RAs No. observations in right ascension --- Ep_RA Epoch of right ascension - 1900.000 ma DE- Declination sign (1950) --- DEd Declination, degrees (1950) deg DEm Declination, minutes (1950) arcmin DEs Declination, seconds (1950) arcsec e_DEs Mean error of declination. arcsec o_DEs No. Observations in declination. --- Ep_DE Epoch of declination. - 1900.000 ma Nancy Grace Roman, J.A. Watko SSDOO/ADC 1995 Dec 27 UNKNOWN UNKNOWN Changes in the catalog as received from the U.S. Naval Observatory have been minor. The false DM number was removed for 1135Z and several bytes were changed to make their meaning more obvious to the user. Bytes 66 - 80 were dropped. In the version received, bytes 66 - 75 were blank and bytes 66 - 80 contained only the second numbers for the stars that had duplicate entries . The spectral types for the stars with composite spectra were obtained from the Henry Draper Catalogue or the Transactions of the Yale University Observatory v.25. We thank Clayton A. Smith for assistance with the preparation of this document. I_161.xml The U.S. Naval Observatory Pleiades Catalog 1163 I/163 US Naval Observatory Pleiades Catalog The U.S. Naval Observatory Pleiades Catalog T C Van Flandern U.S. Naval Observatory, unpublished ??? ??? 1969 1969 I/90 : Positions of 502 Stars in Pleiades Region (Eichhorn et al., 1970) Eichhorn H., Googe W.D., Lukac C.F., Murphy J.K., 1970, Mem. Roy. Astron. Soc. 73, 125 (1970MmRAS..73..125E) (Catalog <I/90>) Hertzsprung E., 1947, Ann. Sterrew. Leiden, 19, 1A Positional data Proper motions Regional catalog This catalog is a special subset of the Eichhorn et al. (1970) Pleiades catalog (see <I/90>) updated to B1950.0 positions and with proper motions added. It was prepared for the purpose of predicting occultations of Pleiades stars by the Moon, but is useful for general applications because it contains many faint stars not present in the current series of large astrometric catalogs.
The catalog cat catalog designation --- ID Sequential P catalog number --- Hertz Hertzsprung (1947) number used in <I/90> Numbers are taken from the catalog of Hertzsprung (1947, Ann. Sterrew. Leiden, 19, 1A) --- m_Hertz Component in visual binary system --- ptv Photovisual magnitude Photovisual magnitudes are taken from the Eichhorn et al. (1970) catalog, rounded off to 0.1m. mag RAh Right Ascension (equinox=B1950, epoch=B1950.0) h RAm Right Ascension B1950.0 min RAs Right Ascension B1950.0 s pmRA Proper motion in RA (B1950.0) Proper motions are given as integers and can be read with format I4, in which case one should divide pmRA and pmDE by 100 to obtain centennial values in seconds of arc. To compute pmRA in seconds of time, the cosine factor must be accounted for, so divide pmRA by 15*cos DE. 0.1mas.yr DE- Sign of declination, B1950.0 --- DEd Declination (equinox=B1950, epoch=B1950.0) deg DEm Declination B1950.0 arcmin DEs Declination B1950.0 arcsec pmDE Proper motion in DE (B1950.0) 0.1mas.yr Wayne H Warren Jr LASP/GSFC/HSTX 1996 Feb 12 I_163.xml The Tokyo PMC Catalog 86: Catalog of Positions of 3974 Stars Observed in 1986 with Tokyo Photoelectric Meridian Circle 1167 I/167 Tokyo Photoelectric Meridian Circle Catalog 1986 The Tokyo PMC Catalog 86: Catalog of Positions of 3974 Stars Observed in 1986 with Tokyo Photoelectric Meridian Circle M Yoshizawa S Suzuki Publ. Nat. Astron. Obs. Japan 1 127 1989 1989PNAOJ...1..127Y I/186 : Tokyo PMC Catalog 85 (Yoshizawa+ 1987) I/187 : Tokyo PMC Catalog 87 (Yoshizawa+ 1991) I/188 : Tokyo PMC Catalog 88 (Yoshizawa+ 1992) I/198 : Tokyo PMC Catalog 89 (Yoshizawa+ 1993) Publications of the National Astronomical Observatory of Japan, Vol. 1, No. 2, pp 127 - 176, 1989. Meridian observations Positional data The second annual catalog of the Tokyo Photoelectric Meridian Circle contains 3974 stars that were observed at least twice between 21 December 1985 and 31 December 1986. Specifically, it contains 1141 FK5 stars, 971 FK4 supplemental stars, 554 AGK3R stars, 403 OB stars, 421 NPZT stars, and 484 SAO stars. The positions are for the mean epoch of observation referred to the equinox and equator of J2000.0 and based on the FK5 system. The internal error of a single observation for the bright stars is 0.24" and 0.27" in right ascension and declination, respectively. The catalog contains, in addition to the positions, the catalog from which the star is taken and the number in that catalog, the mean epoch and number of observations of each component of the position and of the magnitude, the spectral type, the V magnitude, and the DM and AGK3 numbers. It also contains the residuals between the position in this catalog and that in the source catalog and mean errors for each component of the position and of the magnitude. Note that a systematic error of the order of 0.1" exists in the FK5 positions for stars in the declination zone 40 - 60 degrees.
The Tokyo PMC86 Catalogue ID Star Number in the Catalog --- Alt Other Catalogue Name --- otherID Star Number in Other Catalogues --- otherV Visual Magnitude in Other Catalogues mag Sp Spectral Type --- Epoch Mean Epoch of the Observations of RA and Dec --- NObs Number of Observations of R.A. and Dec. --- RAh observed J2000 R.A. at the mean epoch (hours) h RAm observed R.A. at the mean epoch (minutes) min RAs observed R.A. at the mean epoch (seconds) s DE- observed J2000 Dec. at the mean epoch (sign) --- DEd observed Dec. at the mean epoch (degrees) deg DEm observed Dec. at the mean epoch (minutes) arcmin DEs observed Dec. at the mean epoch (seconds) arcsec O-C_RA (O-C) in R.A. at the mean epoch to be added to the Source Catalogue s O-C_DE (O-C) in Dec. at the mean epoch to be added to the Source Catalogue arcsec e_RAs mean error of the observed R.A. s e_DEs mean error of the observed Dec. arcsec EpMag mean epoch of the observations of magnitude a o_Mag number of observations of magnitude --- Mag observed magnitude at the mean epoch mag e_Mag mean error of the observed magnitude mag DM_zone BD or CD zone from PPM Catalog --- DM_no BD or CD number from PPM Catalog --- AGK_zone AGK3 zone --- AGK_no AGK number --- and C.-H. Joseph Lyu; Nancy Roman & Paul Kuin NASA ADC 1997 Jan 09 UNKNOWN UNKNOWN * October 1990: Catalogue received at CDS * 01-Apr-1992: A new documentation (pmc86.doc) was received from the Astronomical Data Analysis Center of the National Astronomical Observatory, Japan. * 20-Feb-1996: Documentation standardized, using the same description as catalog I/198 by S. Nishimura [ADAC/NAOJ], from 01-Sept-1993 * 08-Mar-1996: Documentation also standardized by J. Lyu at NASA/ADC. * 09-Jan-1997: Combined best of both documents. I_167.xml Perth 83, A Catalogue of Positions of 12,263 Stars 1168 I/168 Perth 83 Catalogue of 12263 Stars Perth 83, A Catalogue of Positions of 12,263 Stars D N Harwood Perth Observatory ??? ??? 1990 1990 Meridian observations Positional data Proper motions The catalogue is based on observations of the Meridian Telescope at the Perth Observatory, that were done between the years 1980 and 1987. The intention of the programme has been to produce a catalogue of positions for all stars down to 7th magnitude, between the declinations +40 and -90 degrees. The original programme contained 14702 stars, but this number was reduced due to instrumental breakdowns. The printed catalogue contained 12263 stars, but the mean value of dx exhibited a strong trend due to a systematic effect related to the magnitude. This machine readable version contains 12331 stars, and it was corrected for the systematic error as appears in the following table (to be compared with table 6 of the printed version). Mean value of dx and dy calculated for each magnitude Magnitude Mean dx No. of Stars Mean dy No. of Stars 1.0 0.03 27 -0.05 27 2.0 -0.10 53 0.00 53 3.0 -0.08 96 0.00 96 4.0 0.01 516 -0.00 516 5.0 0.04 1421 0.02 1421 6.0 0.10 4234 -0.02 4234 7.0 0.04 4754 -0.01 4754 8.0 -0.04 990 0.04 990 9.0 0.08 221 0.23 221 10.0 0.39 18 0.03 18
Catalog file Prog Program number --- SpTCode Code for spectral type 8=B0 2=F2 -7=G5 -25=M2 7=B5 1=F5 -12=K0 -26=M3 6=A0 0=F7 -14=K2 -27=M5 5=A5 -1=F8 -17=K5 -28=M7 3=F0 -2=G0 -24=M0 -29=N --- Mv Observed visual magnitude if o_Mv>0 mag e_Mv Std. deviation of the mean of the magnitude mag o_Mv Number of obs. for magnitude determination --- RAh Right ascension hours (1950.0B) h RAm Right ascension minutes (1950.0B) min RAs Right ascension seconds (1950.0B) s DE- Declination sign --- DEd Declination degrees (1950.0B) deg DEm Declination arcmin (1950.0B) arcmin DEs Declination arcsec (1950.0B) arcsec pmRA Annual proper motion in RA s pmDE Annual proper motion in Dec arcmin dRAcosDE Meaned residuals (delta RA X cos DEC) in the sense (O-C) for equinox 1950.0B arcsec dDE Meaned residuals (delta DEC) in the sense (O-C) for equinox 1950.0B arcsec e_dx Standard deviations for the mean dx --- e_dy Standard deviations for the mean dy --- o_dx Numbers of observations for the mean dx --- o_dy Numbers of observations for the mean dy --- RAEpoch Mean epoch of observation for RA and dx yr DEEpoch Mean epoch of observation for DEC and dy yr SAO SAO number --- Fstar Reference star flag "F" means that the star has been used as a reference star. --- PosCorr Positional corrections applied flag "*" means that the star has had parallax and/or radial velocity applied in computing the positions. --- James E. Gass SSDOO/ADC 1997 Jul 23 The author, Harwood acknowledges the collaboration of C. Bowers, S. Ewing, M. Sultana and A. Verveer. I_168.xml A Catalog of Selected Compact Radio Sources for the Construction of an Extragalactic Radio/Optical Reference Frame 1169 I/169 Construction of Extragalactic Reference Frame A Catalog of Selected Compact Radio Sources for the Construction of an Extragalactic Radio/Optical Reference Frame A N Argue C de Vegt B Elsmore J Fanselow R S Harrington P Hemenway K J Johnston H Kuehr I I Kumkova A E Niell H G Walter A Witzel Astron. and Astrophys. 130 191 1984 1984A&A...130..191A Positional data Radio sources This catalog was compiled to provide accurate positions for selected strong, compact extragalactic radio sources proposed for establishing an almost inertial reference frame against which the motions of Earth, galactic objects, and spacecraft may be measured. It is also intended to define sources for which precise optical positions should be determined in order to relate its established reference frame with the fundamental optical system of the FK5. Astrometric data for 233 compact radio sources having identified optical counterparts are given. The data listed for each source are source identification, equatorial position (J2000.0), mean positional errors, object classification (galaxy, BL Lacertae object, QSO), visual magnitude, redshift, 5-GHz flux density, and observation and remarks codes. The data were computerized at the Astronomical Data Center, NASA/GSFC.
Astrometric data for 233 compact radio sources ID Source Identification designation Designation according to the IAU convention, which uses the B1950.0 coordinates of right ascension in hours and minutes followed by the sign and the declination truncated (not rounded) to a tenth of a degree. --- Scode Source code An asterisk denotes a source south of declination -45deg. having a preliminary position from a joint CSIRO-JPL program (Jauncey et al. 1982). --- Alt Alternate source name Names from other catalogs or lists by which a source is commonly known. --- RAh Right ascension hours (equinox J2000) Weighted means of the right ascension and declination at equinox J2000.0. The weights assigned were inversely proportional to the squares of the quoted errors in position. Individual catalog positions that were presented at equinox B1950.0 were precessed to J2000.0 using the procedure described by Kaplan (1981). Epochs of observation used to precess the coordinates to J2000.0 were those given in the respective publications. The epochs, reference equinoxes, and adjustments made to the right ascension origins of individual catalogs are listed in Table 1 of the source reference. h RAm right ascension minutes min RAs right ascension seconds s e_RAs Error in right ascension Standard errors of the mean positions in right ascension and declination, taken as the greater of either the internal or external errors of the standard error of the mean. A right ascension error is not given for the source 3C 273 (1226+023) because the zero point in right ascension has been set to the position of 3C 273B reported by Hazard et al. (1971), which is defined here for J2000.0 as 12h 29m 06s. s DE- Sign of declination zone --- DEd Declination degrees (equinox J2000) deg DEm DEC arc minutes arcmin DEs DEC arc seconds arcsec e_DEs Error in declination arcsec NCat Number of catalogs used for averaging The number of different catalogs used to obtain the weighted mean. --- ObjClass Optical Classification code A code letter to specify the optical identification of the object, as follows: G = galaxy L = BL Lacertae object Q = quasar E = ? = A question mark denotes uncertainty. --- V Visual magnitude The visual magnitude, as taken from any of a variety of sources. mag u_z Left parenthesis for uncertain z value --- z Redshift Sources are not given for redshift values. A value is surrounded by parentheses in bytes 75 and 81 if the z datum is uncertain. --- Rparen Right parenthesis for uncertain z value --- F(5GHz) 5-GHz flux density As measured with the VLA. It is the flux density of the entire source and the epoch of measurement is 1979. Jy ObsCode Observation code The codes given in the source reference are as follows: A = source observed by the VLA and JPL P = primary VLA calibrator S = secondary VLA calibrator However, only the A code is present in the published catalog. --- RemCode Remark code A lower case letter for a remark listed following the published table: a = nebulous extension b = extended H II c = optical double d = optical multiple e = optically diffuse f = nebulous (POSS E plate) g = diffuse (POSS O plate) --- N. G. Roman, C.-H. Lyu, N.P.M. Kuin Hughes STX/NASA 1996 Apr 04 UNKNOWN UNKNOWN The candidate sources were selected from a number of astrometric and survey reference catalogs that are listed in Table 1 of the source reference. Six sources south of declination -45 deg. were included from Jauncey et al. (1982). All selected sources display little or no spatial structure at the arcsecond level Four of the sources listed in the catalog have subsequently been dropped because they show unacceptable structure (Kumkova, I. I. 1990, private communication) and have flat or complex radio spectra. The accuracy of the radio positions of the catalog sources is <= 0.1 arc seconds, with the majority <= 0.01". Additional observations are expected to refine the positions to <= 0.005". It is expected that the machine- readable version of the catalog will be updated from time to time as improved positions become available. For additional information concerning the reasons for the preparation of the catalog, the selection of candidate radio sources, and the distribution of sources over the sky, the source reference should be consulted. I_169.xml Astrographic Catalogue Reference Stars 1171 I/171 Astrographic Catalog Reference Stars Astrographic Catalogue Reference Stars T E Corbin S E Urban W H Warren Jr. NASA, NSSDC 91-10 ??? ??? 1991 1991 I/15 : FK4 Catalogue (Fricke and Kopff, 1963) I/72 : AGK3R Catalogue (Corbin, 1978) I/85 : CPC2 (2nd Cape Photographic Catalogue 1950, Nicholson et al., 1984) I/172 : IRS (International Reference Stars, Corbin, 1991) I/149 : FK5 Catalogue (Fricke et al., 1988, Veroff. ARI 32) I/219 : Cape AC Zone (-41 to -51) Reduced to ACRS (Urban & Corbin, 1995) I/222 : San Fernando AC Zone (-3 to -9) (Urban et al., 1995) I/223 : Algiers AC Zone (+4 to -2) Reduced to ACRS (Urban et al., 1995) Corbin, T.E., and Urban, S.E. 1989, in Star Catalogues: A Centennial Tribute to A. N. Vyssotsky (Schenectady, L. Davis Press), p. 59 de Vegt, Ch., Zacharias, N., Murray, C.A., and Penston, M.J. 1989, in Star Catalogues: A Centennial Tribute to A. N. Vyssotsky (Schenectady, L. Davis Press), p. 45 (Catalog: <I/85>) Schwan, H., =1988A&A...198..363S Positional data Proper motions The ACRS is an all-sky catalog of positions and proper motions that is based on the AGK3 in the north and on the newly completed second Cape Photographic Catalogue (CPC2, de Vegt et al. 1989) in the south. The astrometric data are on the system of the International Reference Stars (IRS, catalog <I/172>), compiled on B1950.0 FK4 and then transformed to J2000.0 FK5. The ACRS contains 320,111 stars, the mean positions for which were derived from a total of 1,643,783 individual input positions. The catalog is divided into two parts. Part 1 contains stars having better observational histories and, therefore, more reliable positions and proper motions, while the stars in Part 2 have poor histories and consist mostly of objects for which only two catalog positions in one or both coordinates were available for computing proper motions. For Part 1, which consists of 78 percent of the catalog, the mean errors of the proper motions in right ascension and declination are 0.47 and 0.46 seconds of arc/century (4.7 and 4.6 mas/yr), respectively. It is intended that, as more observations are accumulated for stars in Part 2, they will be migrated to Part 1. The catalog was compiled at the U.S. Naval Observatory, Washington, D.C., for purposes of performing new reductions of the Astrographic Catalogue plates. Additional details about the construction of the ACRS may be found in Corbin and Urban (1989). The data included are catalog part, ACRS number, equatorial coordinates (equinox, equator, epoch B1950.0 and J2000.0), proper motions (B1950.0 and J2000.0), original epochs, weights for right ascension and declination, and reference data such as DM numbers (BD, CD, CPD), AGK3 and CPC2 designations, and an IAU recommended ACRS identifier (based on coordinates).
Part 1: more reliable stars Part 2: stars with poor observational history PartNum Catalog Part number, '1' or '2' --- ACRS ACRS sequential number This number is between 1 and 250052 for the first part, between 500001 and 570159 for Part 2. --- RAh Hours RA, equinox=B1950, Epoch=B1950.0 h RAm Minutes RA, equinox, epoch B1950.0 min RAms Seconds RA, equinox, epoch B1950.0 ms DE- Sign Dec, equinox, epoch B1950.0 --- DEd Degrees Dec, equinox, epoch B1950.0 deg DEm Minutes Dec, equinox, epoch B1950.0 arcmin DEcs Seconds Dec, equinox, epoch B1950.0 10mas e_RAms Mean error in RA at original epoch ms e_DEcs Mean error in Dec at original epoch 10mas pmRA RA proper motion, FK4 system 0.01ms/yr pmDE DE proper motion, FK4 system 0.1mas/yr e_pmRA Mean error on pmRA 0.01ms/yr e_pmDE Mean error on pmDE 0.1mas/yr EpRA Original epoch of RA (epoch mean position) 0.001yr EpDE Original epoch of DE (epoch mean position) 0.001yr o_RAms Number of positions in RA --- o_DEcs Number of positions in DE --- w_RAms Sum of the weights in RA 0.1 w_DEcs Sum of the weights in DE 0.1 Pmag Photographic magnitude 0.01mag SpType Spectral type --- BD Bonner Durchmusterung number <I/122> --- CD Cordoba Durchmusterung number <I/114> --- CP Cape Photographic Durchmusterung <I/108> --- AGK3 AGK3 number <I/61> --- CPC2 Second Cape Photograpic Catalog <I/85> --- ACRSJ ACRS number, ACRS Jhhmmss.ssSddmmss.s This identifier is based upon the recommended IAU nomenclature (see PASP, 102, 1444, 1990). The field consists of an origin in bytes 127-130 (ACRS) and a coordinate specification in bytes 132-150 (byte 132 contains a "J" to indicate that the following coordinates are in the Julian reference system and are for the year 2000.0, the standard equinox designated for Julian system coordinates). --- RA2000h Hours RA, Equinox=J2000, Epoch=J2000 The J2000 positions are given for equinox and epoch J2000.0 on the system of FK5 after transformation of the B1950.0 values. The transformation was done using the coefficients and software package of Schwan (see Schwan 1988) and the algorithm given in the 1991 Astronomical Almanac (page B42) (foreshortening terms set to zero). (See Section 3.1 of the documentation for additional details.) h RA2000m Minutes RA, equinox, epoch J2000.0 min RA2000ms Seconds RA, equinox, epoch J2000.0 ms pmRA2000 Centennial RA proper motion, J2000.0 0.01ms/yr EpRA-J2000 Original epoch - J2000.0 in RA These values are wrong for values larger than 1 century (when the corresponding epoch is before 1900); this occurs for ACRS 86508, 240650, 533151. 0.001yr DE2000- Sign Dec, equinox, epoch J2000.0 --- DE2000d Degrees Dec, equinox, epoch J2000.0 deg DE2000m Minutes Dec, equinox, epoch J2000.0 arcmin DE2000cs Seconds Dec, equinox, epoch J2000.0 10mas pmDE2000 Centennial Dec proper motion, J2000.0 0.1mas/yr EpDE-J2000 Original epoch - J2000.0 in DE 0.001yr acrs.doc ASCII documentation acrs.tex LaTeX documentation Gail L. Schneider SSDOO/ADC Francois Ochsenbein CDS 1995 Nov 29 UNKNOWN UNKNOWN * 03-Apr-1991: the completed machine-readable ACRS was transferred to the Astronomical Data Center (NASA/Goddard) * Catalogue distributed on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1991), directory /astrom/acrs * 29-Nov-1995: data files checked, and ReadMe file standardized at CDS I_171.xml International Reference Stars (IRS) 1172 I/172 International Reference Stars International Reference Stars (IRS) T E Corbin W H Warren Jr. NASA, NSSDC 91-11 ??? ??? 1991 1991 I/15 : FK4 Catalogue (Fricke and Kopff, 1963) I/72 : AGK3R Catalogue (Corbin, 1978) I/85 : CPC2 (2nd Cape Photographic Catalogue 1950, Nicholson et al., 1984) I/138 : SRS (Southern Reference Star catalogue, Smith, 1988) I/149 : FK5 Catalogue (Fricke et al., 1988, Veroff. ARI 32) I/146 : PPM-North (Roeser and Bastian, 1988) I/193 : PPM-South (Bastian and Roeser, 1993) Corbin, T.E. 1977, The Proper-Motion System of the AGK3R (Ann Arbor, University Microfilms, Inc.) Corbin, T.E. 1978, in IAU Colloquium 48, Modern Astrometry, ed. F.V. Prochazka and R.H. Tucker (Vienna, University Obs.), p. 505 (Catalog <I/72>) Fricke, W., and Kopff, A. 1963, "Fourth Fundamental Katalog (FK4)", Veroeff. Astron. Rechen-Inst. Heidelb. No. 10 (Catalog <I/15>) Schwan, H., =1988A&A...198..363S Smith, C.A., Corbin, T.E., Hughes, J.A., Jackson, E.S., Krutskaya, E.V., Polozhentsev, A.D., Polozhentsev, D.D., Yagudin, L.I., and Zverev, M.S. 1990, in IAU Symposium No. 141, Inertial Coordinate System on the Sky, ed. J.H. Lieske and V.K. Abalakin (Dordrecht, Reidel), p.457 (Catalog <I/138>) Positional data Proper motions The IRS is an all-sky catalog of positions and proper motions that is based on the AGK3R (Corbin 1977, 1978) in the Northern Hemisphere and on the newly completed SRS (Smith et al. 1990) in the south. The data for the 36027 stars of the IRS were compiled in B1950.0 FK4 and then transformed to J2000.0 FK5. The IRS was compiled by matching 122 meridian circle catalogs with the AGK3R and SRS to provide the data base. Catalogs whose stars had been observed using screens to minimize the magnitude equation and that contained FK4 (Fricke and Kopff 1963) stars were used to form a preliminary system. These catalogs were reduced to the FK4 by direct comparison; the resulting positions and proper motions were then used to reduce all of the other catalogs. Thus, the IRS is a differential catalog compiled from 164,917 positions reduced to the FK4 system. The IRS is divided into two parts. Part 1 contains the stars having better observational histories and, therefore, more reliable positions and proper motions. This part constitutes 81 percent of the catalog; mean errors of the proper motions are 0.43 and 0.44 seconds of arc/century (4.3 and 4.4 mas/yr) in right ascension and declination, respectively. The stars in Part 2 have poor observational histories and consist mostly of objects for which only two catalog positions in one or both coordinates were available when the proper motions were computed. Where accuracy is the primary consideration, it is best to use only the stars in Part 1, while if the highest possible density is desired, the two parts should be combined, as they are systematically the same. The data included are catalog part, IRS number, equatorial coordinates (equinox, equator, epoch B1950.0 and J2000.0), centennial proper motions (B1950.0 and J2000.0), original epochs, weights for right ascension and declination, and reference data such as DM numbers (BD, CD, CPD), AGK3 and CPC2 designations, and an IAU-recommended IRS identifier (based on coordinates).
Part 1: more reliable positions and proper motions Part 2: stars with poor observational history PartNum Catalog Part number, '1' or '2' --- IRS IRS sequential number This number is between 1 and 29163 for the first part, between 70001 and 76865 for Part 2. --- RAh Hours RA, equinox=B1950, Epoch=B1950.0 h RAm Minutes RA, equinox, epoch B1950.0 min RAms Seconds RA, equinox, epoch B1950.0 ms DE- Sign Dec, equinox, epoch B1950.0 --- DEd Degrees Dec, equinox, epoch B1950.0 deg DEm Minutes Dec, equinox, epoch B1950.0 arcmin DEcs Seconds Dec, equinox, epoch B1950.0 10mas e_RAms Mean error in RA at original epoch ms e_DEcs Mean error in Dec at original epoch 10mas pmRA RA proper motion, FK4 system 0.01ms/yr pmDE DE proper motion, FK4 system 0.1mas/yr e_pmRA Mean error on pmRA 0.01ms/yr e_pmDE Mean error on pmDE 0.1mas/yr EpRA Original epoch of RA (epoch of mean position) 0.001yr EpDE Original epoch of DE (epoch of mean position) 0.001yr o_RAms Number of positions in RA --- o_DEcs Number of positions in DE --- w_RAms Sum of the weights in RA 0.1 w_DEcs Sum of the weights in DE 0.1 Pmag Photographic magnitude 0.01mag SpType Spectral type --- BD Bonner Durchmusterung number <I/122> --- CD Cordoba Durchmusterung number <I/114> --- CP Cape Photographic Durchmusterung <I/108> --- AGK3 AGK3 number <I/61> --- CPC2 Second Cape Photograpic Catalog <I/85> --- IRSJ IRS number, IRS Jhhmmss.ssSddmmss.s This identifier is based upon the recommended IAU nomenclature (see PASP, 102, 1444, 1990). The field consists of an origin in bytes 127-130 (IRS) and a coordinate specification in bytes 132-150 (byte 132 contains a "J" to indicate that the following coordinates are in the Julian reference system and are for the year 2000.0, the standard equinox designated for Julian system coordinates). Bytes 127 and 131 are blank for this catalog. --- RA2000h Hours RA, Equinox=J2000, Epoch=J2000 The J2000 positions are given for equinox and epoch J2000.0 on the system of FK5 after transformation of the B1950.0 values. The transformation was done using the coefficients and software package of Schwan (see Schwan 1988) and the algorithm given in the 1991 Astronomical Almanac (page B42) (foreshortening terms set to zero). (See Section 3.1 of the documentation for additional details.) h RA2000m Minutes RA, equinox, epoch J2000.0 min RA2000ms Seconds RA, equinox, epoch J2000.0 ms pmRA2000 Centennial RA proper motion, J2000.0 0.01ms/yr EpRA-J2000 Original epoch - J2000.0 in RA 0.001yr DE2000- Sign Dec, equinox, epoch J2000.0 --- DE2000d Degrees Dec, equinox, epoch J2000.0 deg DE2000m Minutes Dec, equinox, epoch J2000.0 arcmin DE2000cs Seconds Dec, equinox, epoch J2000.0 10mas pmDE2000 Centennial Dec proper motion, J2000.0 0.1mas/yr EpDE-J2000 Original epoch - J2000.0 in DE 0.001yr irs.doc ascii documentation irs.tex LaTeX documentation Gail L. Schneider SSDOO/ADC Francois Ochsenbein CDS 1995 Nov 29 UNKNOWN UNKNOWN * 16-Apr-1991: the completed machine-readable IRS was transferred to the Astronomical Data Center (NASA/Goddard) * Catalogue distributed on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1991), directory /astrom/irs * 29-Nov-1995: ReadMe file standardized at CDS I_172.xml Fifth Fundamental Catalogue (FK5) Part II. The FK5 Extension 1175 I/175 Fifth Fundamental Catalogue Fifth Fundamental Catalogue (FK5) Part II. The FK5 Extension W Fricke H Schwan T E Corbin U Bastian R Bien C Cole R Jackson R Jaehrling H Jahreiss T Lederle S Roeser Veroeff. Astron. Rechen-Institut Heidelb. No. 33, ??? ??? 1991 1991VeARI..33....1F I/49 : Part I: Basic Fundamental Stars Corbin, T. E. 1978, in IAU Colloquium 48, Modern Astrometry, ed. F. V. Frochazka and R. H. Tucker (Vienna, University Obs.), p. 505 Fricke, W., and Kopff, A. 1963, Fourth Fundamental Katalog (FK4), Veroeff. Astron. Rechen-Institut Heidelb. No. 10. (Catalogue <I/143>) Fricke, W., Schwan, H., and Corbin, T. (in collaboration with Bastian, U., Bien, R., Cole, C., Jackson, R., Jaehrling, R., Jahreiss, H., Lederle, T., and Roeser, S.) 1991, Fifth Fundamental Catalogue FK5), Part II. The FK5 Extension, New Fundamental Stars, Veroeff. Astron. Rechen-Institut Heidelburg No. 33 Fricke, W., Schwan, H., and Lederle, T. (in collaboration with Bastian, U., Bien, R., Burkhardt, G., du Mont, B., Hering, R., Jaehrling, R., Jahreiss, H., Roeser, S., Schwerdtfeger, H. M., and Walter, H. G.) 1988, Fifth Fundamental Catalogue (FK5), Part I. The Basic Fundamental Stars, Veroeff. Astron. Rechen-Institut Heidelburg No. 32, catalog <I/149> Lieske, J. H. 1979, A&A, 73, 282 Scott, F. P., and Smith, C. A., Jr. 1971, Comparison of the SAO and AGK3R Star Catalogues, in Conference on Photographic Astrometric Techniques, ed. H. K. Eichhorn, NASA CR-1825, catalog <I/161> Smith, C. A., Corbin, T. E., Hughes, J. A., Jackson, E. S., Krutskaya, E. V., Polozhentsev, A. D., Polozhentsev, D. D., Yagudin, L. I., and Zverev, M. S. 1990, in IAU Symposium No. 141, Inertial Coordinate System on the Sky, ed. J. H. Lieske and V. K. Abalakin (Dordrecht, Reidel), p. 457 Positional data Proper motions The FK5 Extension provides improved mean positions and proper motions for the 3117 new fundamental stars. The machine version of the catalog contains the positions and proper motions of the Extension stars for the epochs and equinoxes J2000.0 and B1950.0, the mean epochs of individual observed right ascensions and declinations used to determine the final positions, the mean errors of the final positions and proper motions for the reported epochs, and ancillary data such as magnitudes, spectral types, parallaxes, and radial velocities. Cross identifications to the numbering systems of the AGK3R, SRS, HD, DM, and GC catalogs are also included.
The Fifth Fundamental Catalogue (FK5) Part II (which may be referred to by the alternate name FK5 Extension) provides mean positions and proper motions at equinox and epoch J2000.0 for 3117 new fundamental stars. The purpose of the FK5, Part II, is mainly to extend the fundamental system defined by the FK5, Part I (the so-called Basic FK5; Fricke et al. 1988) to about magnitude 9.5. The positions and proper motions given in the FK5 Extension are in accordance with the IAU (1976) system of astronomical constants; this means that the proper motions are based on the new values for the precessional quantities, the terms of elliptic aberration are eliminated from the mean positions, the correction for the error in the FK4 equinox and its fictitious motion are applied, and the systematic corrections FK5-FK4, as given in the Basic FK5 (page 86), have been taken into account. More than 200 catalogs providing star positions obtained from throughout the world have been used in the compilation of the FK5 Extension. The source reference should be consulted, along with the FK5 Basic catalog (Fricke et al. 1988) for more detailed information regarding the motivation for construction of the FK5, the determination of its equator and equinox, the expressions for general precession, a discussion of the FK5 system, systematic differences between the FK4 and FK5, the transformation of observational catalogs to the FK5 system and to the reference system J2000.0, and more thorough descriptions of the data contained in the FK5 catalog. In fact, the source reference should be consulted by all users before utilizing the FK5 data for astrometric applications. The trigonometric parallax and radial velocity fields are blank when data are missing, and because parallax and radial velocity can validly be zero, the fields should be checked for blanks before the data are used. The user should note that the file is ordered by FK5 number, which means that the stars are arranged neither by right ascension nor by declination.
FK5 Extension - Part II FK5 FK5 Extension number These numbers begin at 2000 (the first is 2003) to distinguish them from the numbers in the Basic FK5. --- RAh Right ascension J2000.0 (hours) Equinox=J2000, Epoch=J2000 The terms of elliptic aberration have been eliminated from the mean positions. The B1950.0 data have been computed from the J2000.0 data using a procedure described in the source reference based on the IAU (1976) system of astronomical constants (see also Lieske 1979). h RAm Right ascension J2000.0 (minutes) min RAs Right ascension J2000.0 (seconds) s pmRA Centennial proper motion J2000.0 Centennial values for J2000.0 and B1950.0, referred to one Julian century. s/ha DE- Declination, J2000.0 (sign) --- DEd Declination, J2000.0 (degrees) Equinox=J2000, Epoch=J2000 deg DEm Declination J2000.0 (minutes) arcmin DEs Declination J2000.0 (seconds) arcsec pmDE Centennial proper motion J2000.0 arcsec/ha RAh1950 Right ascension B1950.0 (hours) Equinox=B1950, Epoch=B1950 h RAm1950 Right ascension B1950.0 (minutes) min RAs1950 Right ascension B1950.0 (seconds) s pmRA1950 Centennial proper motion B1950.0 s/ha DE-1950 Declination B1950.0 (sign) --- DEd1950 Declination B1950.0 (degrees) Equinox=B1950, Epoch=B1950 deg DEm1950 Declination B1950.0 (minutes) arcmin DEs1950 Declination B1950.0 (seconds) arcsec pmDE1950 Centennial proper motion B1950.0 arcsec/a2 EpRA Epoch (RA) Mean epoch (-1900.0) of the individual observed right ascensions and declinations. a e_RAs Mean error in RA These mean errors do not include those of the FK5 system and of the equinox and equator. ms e_pmRA Mean error in centennial PM ms/ha EpDE Epoch (Dec) a e_DEs Mean error in Dec 10mas e_pmDE Mean error in centennial PM 10mas/ha Vmag V magnitude For physical double stars, the magnitudes of the brighter components are given (both are given in the published catalog). mag n_Vmag Magnitude flag 'V' indicates that a range of magnitudes is given in the published catalog. 'v' indicates variability (amplitude exceeds 0.3 magnitude). --- Sp Spectral type(s) --- plx Parallax arcsec RV Radial velocity km/s AGK3R AGK3R (catalog <I/161>) number Only three stars (1367, 1553, 1598) in the Basic FK5 have this number. --- SRS SRS (catalog <I/138>) number --- HD HD (catalog <III/135>) number --- DM DM identification BD = Bonner Durchmusterung (Argelander 1859-62, Kuestner 1903 <I/122>) SD = Southern Durchmusterung (Schoenfeld 1886 <I/119>) CD = Cordoba Durchmusterung (Thome 1892- 1932 <I/114>) CP = Cape Photographic Durchmusterung (Gill and Kapteyn 1895-1900 <I/108>) --- GC GC (catalog <I/113>) number --- Nancy G. Roman NSSDC/ADC 1994 Dec 08 Dr. H. Schwan and his colleagues at the Astronomisches Rechen-Institut generously reviewed a draft copy of the original documentation prior to its final release for distribution with machine-readable copies of the catalog, as did Dr. T. E. Corbin of the U. S. Naval Observatory. Dr. Warren prepared the original document which has been reformatted here in the new standard form. UNKNOWN UNKNOWN The machine-readable Fifth Fundamental Catalogue (FK5) Part II was received on magnetic tape from Dr. H. Schwan of the Astronomisches Rechen-Institut, Heidelberg on 19 August 1991. The logical record length of the catalog, as received, was 220 bytes. The following format changes were made by Wayne H. Warren Jr., (with Dr. Schwan's concurrence) in order to make the data easier to interpret and to conserve storage: 1. The DM identifiers, which were single-digit numerical codes, were changed to "BD", "CD", and "CP". 2. Plus signs were added to the trigonometric-parallax data, even though no negative parallaxes are included in the catalog, to indicate that negative parallaxes are possible. 3. Multiple blanks between data fields were removed, as were blanks beyond the end of each record, to decrease the logical record length from 220 bytes to 190 bytes. 4. Byte 129 (the variability flag) had only upper case "V" flags as received. These were left for cases where magnitude ranges are given in the published catalog, but were changed to lower case when a lower case "v" is reported in the published edition. I_175.xml The AGK3U: an updated version of the AGK3 1176 I/176 AGK3U The AGK3U: an updated version of the AGK3 B Bucciarelli D Daou M G Lattanzi L G Taff Astron. J. 103 1689 1992 1992AJ....103.1689B I/69 : AGK3 Catalog I/146 : Catalog of Positions and Proper Motions (PPM-North), with improved data for Northern stars I/220 : The Guide Star Catalog (GSC), V1.1 Positional data Proper motions The AGK3U is a updated version of the AGK3 catalog in which new positions from the Palomar "Quick V" survey have been added to improve the AGK3 proper motions. It provides FK4/B1950.0 positions and proper motions for 170,464 stars north of -2.5 degrees declination, at an average epoch of 1950.62. The proper motions have a two dimensional formal mean error of 0.82 arcsec/century. In addition to the positions and proper motions, the catalog contains the AGK3 number, the mean errors of the positions and proper motion in each coordinate, the photographic magnitude, the spectral type, and the Palomar plate position, epoch, and mean error.
*The AGK3U Catalogue AGK3 AGK3 Number number=1 the AGK3 number (identical to AGK2) is made of byte #2: Zone sign ("+" or "-") bytes #3-4: the Zone (degree of declination) bytes #5-8: number within zone (zero filled) --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec e_RAs Mean error of right ascension*cos(delta). arcsec e_DEs Mean error of the declination. arcsec pmRA Proper motion in RA (* cos(delta)) number=2 the proper motions are expressed in arcsec per tropical century. 10mas/yr pmDE Proper motion in declination number=2 the proper motions are expressed in arcsec per tropical century. 10mas/yr e_pmRA Mean error of pmRA number=2 the proper motions are expressed in arcsec per tropical century. 10mas/yr e_pmDE Mean error of pmDE number=2 the proper motions are expressed in arcsec per tropical century. 10mas/yr EpRA Mean epoch for the right ascension number=3 in tropical years. yr EpDE Mean epoch for the declination number=3 in tropical years. yr Model Model flag number=4 the model flag is 0 when a linear model was used for the determination of proper motion; the model flag is 1 to 8 when the linear model failed the chi-square testing. --- --- Always a dot. --- s0RA sigma zero of least square solution in RA. --- s0DE sigma zero of least square solution in Dec. --- mpg Photographic magnitude from PPM <I/146> mag Sp Spectral type from the PPM <I/146> --- Type Type of adopted solution number=5 the symbols used for the model are: s: subplate m: mask --- RAhGSC Right Ascension B1950 in GSC (hours) h RAmGSC Right Ascension B1950 in GSC (minutes) min RAsGSC Right Ascension B1950 in GSC (seconds) s DE-GSC Declination B1950 in GSC (sign) - DEdGSC Declination B1950 in GSC (degrees) deg DEmGSC Declination B1950 in GSC (minutes) arcmin DEsGSC Declination B1950 in GSC (seconds) arcsec EpGSC Epoch of GSC observation number=3 in tropical years. yr ErrGSC Mean error per coordinate in GSC arcsec Francois Ochsenbein CDS 1996 Nov 05 I_176.xml The Second General Catalogue of Stars Observed with the Photoelectric Astrolabes (GCPA2) 1181 I/181 Second General Catalogue of Stars The Second General Catalogue of Stars Observed with the Photoelectric Astrolabes (GCPA2) L Lu Bull. Inf. CDS 40 9 1992 1992BICDS The Second General Catalogue of Stars Observed with the Photoelectric Astrolabes (GCPA2) L Lu Publ. of the Beijing Astron. Obs., No. 17 ??? ??? 1991 1991PBeiO..17....1L Fundamental catalog Positional data Stars, fundamental On the basis of the data observed with the photoelectric astrolabes in China observed during the period from 1982 to 1990, the Second general cata- logue of stars have been compiled. With magnitudes ranging from 0.1 to 7.3, the general catalogue consists of 2606 stars. The declination are from -3 degree to +69 degree. In the catalogue there are 980 FK5 stars and 1626 GC stars. The mean precisions of position corrections in right ascension and declination are 3.8 ms and 0.064", respectively. The mean epoch of the catalogue is 1988.0.
Catalog Data FK5 Number of FK5 or FK4supp or GC Number of FK5 or FK4supp or GC after 980 records (record 981 is blank) --- mag Visual magnitude mag Sp Spectral type --- RAh += Right Ascension J2000.0 hours Equator and Equinox of J2000.0 h RAm Right Ascension J2000.0 minutes Equator and Equinox of J2000.0 min RAs Right Ascension J2000.0 seconds Equator and Equinox of J2000.0 s DE- Declination J2000.0 sign --- DEd Declination J2000.0 degrees deg DEm Declination J2000.0 arcminutes arcmin DEs Declination J2000.0 arcseconds arcsec corRA Position correction of RA at EpRA Equator and Equinox of J2000.0 ms e_corRA Mean error of the correction on RA Equator and Equinox of J2000.0 ms EpRA Mean epoch of observation on RA (-1900) Equator and Equinox of J2000.0 a corDE Position correction of DE at EpDE 0.01as e_corDE Mean error of the correction on DE 0.01as EpDE Mean epoch of observation on DE (-1900) a Julie Anne Watko SSDOO/ADC 1996 Aug 15 The content of this ReadMe is from an unsigned Intro file (25-Feb-1992). It was modified to the current CDS standard at ADC by J.A. Watko (MAY-1996). UNKNOWN UNKNOWN by exchange from Beijing I_181.xml Fourth Preliminary Catalogue of Stars Observered with the Photoelectric Astrolabe (PACP4) 1182 I/182 Fourth Preliminary Catalogue of Stars Fourth Preliminary Catalogue of Stars Observered with the Photoelectric Astrolabe (PACP4) L Lu CDS Bull. No. 40, p. 11 ??? ??? 1992 1992BICDS Fourth Preliminary Catalogue of Stars Observered with the Photoelectric Astrolabe (PACP4) L Lu Pub. Beijing Astron. Obs., No. 17 ??? ??? 1991 1991PBeiO..17...59L Fundamental catalog Stars, fundamental Using the data observed with the Photoelectric Astrolabe Mark II of the Beijing Astronomical Observatory (PPA) during the period from 1982 to 1990, the Fourth Preliminary Catalogue of Stars (PACP4) has been Compiled. It consists of 1969 stars including 650 FK5 stars and 1319 GC stars. The mean precisions of position corrections in right ascension and declination are 4.1 ms and 0.067", respectively. The declinations are from +11 deg to +69 deg. The magnitudes are from 0.1 to 7.3. The mean epoch of observations is 1986.8.
Fourth Preliminary Catalogue of Stars Data PACP4 Serial Number of the PACP4 --- FK5 Number in FK5 or FK4supp or GC The number in this field is FK5 or FK4 supplement number in first 650 records and GC number after 650 records --- mag Visual magnitude mag Sp Spectral type --- RAh Right Ascension (J2000.0) hours Coordinates for Equator and Equinox of J2000.0. h RAm Right Ascension (J2000.0) minutes min RAs Right Ascension (J2000.0) seconds s DEd Declination (J2000.0) degrees deg DEm Declination (J2000.0) arcminutes arcmin DEs Declination (J2000.0) arcseconds arcsec corRA Position correction RA, mean epoch of obs. ms e_corRA Mean error of corRA ms corDE Position correction DE, mean epoch of obs. 10-2as e_corDE Mean error of the corDE 10-2as N Number of observations --- Ep Mean epoch of observation (yr-1900) a UNKNOWN 1992 standardized Julie Anne Watko [SSDOO/ADC] 12-Aug-1996 Feb 25 I_182.xml The Tokyo PMC Catalog 85: Catalog of Positions of 1007 Stars Observed in 1985 with Tokyo Photoelectric Meridian Circle 1186 I/186 Tokyo Photoelectric Meridian Circle Catalog 1985 The Tokyo PMC Catalog 85: Catalog of Positions of 1007 Stars Observed in 1985 with Tokyo Photoelectric Meridian Circle M Yoshizawa S Suzuki R Fukaya Ann. Tokyo Astron. Obs., Univ. Tokyo 2nd Ser. 21 399 1987 1987AnTok..21..399Y I/167 : Tokyo PMC Catalog 86 (Yoshizawa+ 1989) I/187 : Tokyo PMC Catalog 87 (Yoshizawa+ 1991) I/188 : Tokyo PMC Catalog 88 (Yoshizawa+ 1992) I/198 : Tokyo PMC Catalog 89 (Yoshizawa+ 1993) Meridian observations Positional data The catalog of positions of 1007 stars (792 FK4 and FK4S stars, 57 OB stars, 49 NPZT stars, and 109 SAO stars) is presented. They were observed during the period from December 1984 to September 1985 with the Tokyo Photoelectric Meridian Circle (Tokyo PMC). The positions in the catalog are referred to the equinox and equator of J2000, and are based on the FK4 system. The internal errors of a single observation were estimated to be (epsilon(alpha)*cos(delta), epsilon(delta)) = (0.16", 0.19"), whereas the mean internal errors of the catalog positions were (0.08", 0.08") for FK4 stars and (0.09", 0.11") for FK4S stars. The comparison of the positions of the FK4 stars in the present catalog with those of the FK4 catalog shows the significant differences delta(alpha(delta)) and delta(delta(delta)) in some declination zones. Some of those differences are commonly found in other recent catalogs. Thus they may be considered to be the real systematic errors in the FK4 system. Neither significant magnitude nor color equation exists in the Tokyo PMC85 catalog.
The Tokyo PMC85 Catalogue N sequence number in the Catalog --- Cat other catalogue name --- otherN star number in other catalogues --- otherMag visual magnitude in other catalogues mag Sp spectral type --- Epoch mean epoch of the observations of R.A. and Dec a Nobs number of observations of R.A. and Dec. --- RAh observed J2000 R.A. at the mean epoch (hours) h RAm observed R.A. at the mean epoch (minutes) min RAs observed R.A. at the mean epoch (seconds) s DE- observed J2000 Dec. at the mean epoch (sign) --- DEd observed Dec. at the mean epoch (degrees) deg DEm observed Dec. at the mean epoch (minutes) arcmin DEs observed Dec. at the mean epoch (seconds) arcsec O-C_RA (O-C) in R.A. at the mean epoch to be added to the Source Catalogue s O-C_DE (O-C) in Dec. at the mean epoch to be added to the Source Catalogue arcsec e_RAs mean error of the observed R.A. s e_DEs mean error of the observed Dec. arcsec EpMag mean epoch of the observations of magnitude a o_Mag number of observations of magnitude --- Mag observed magnitude at the mean epoch mag e_Mag mean error of the observed magnitude mag DM BD or CD numbers taken from PPM Catalog --- AGK AGK3 numbers --- CDS 1996 Feb 20 UNKNOWN UNKNOWN * 30-Sep-1991: the catalogue was supplied to CDS by Shiro Nishimura; the reformatting of the data were carried out at the Astronomical Data Analysis Center of the National Astronomical Observatory, Japan. * 20-Feb-1996: Documentation standardized, using the same description as catalog I/198 by S.Nishimura [ADAC/NAOJ], from 01-Sept-1993 I_186.xml Catalog of positions of 5748 stars observed in 1987 with Tokyo Photoelectric Meridian Circle (PMC87) 1187 I/187 Tokyo Photoelectric Meridian Circle Catalog 1987 Catalog of positions of 5748 stars observed in 1987 with Tokyo Photoelectric Meridian Circle (PMC87) M Yoshizawa S Suzuki Publ. National Astron. Obs. Japan 2 103 1991 1991PNAOJ...2..103Y I/186 : Tokyo PMC Catalog 85 (Yoshizawa+ 1987) I/167 : Tokyo PMC Catalog 86 (Yoshizawa+ 1989) I/188 : Tokyo PMC Catalog 88 (Yoshizawa+ 1992) I/198 : Tokyo PMC Catalog 89 (Yoshizawa+ 1993) Meridian observations Positional data The third annual catalog of the Tokyo PMC is presented for 5748 stars which had been observed at least two times in the year 1987 period, that is, from January 1, 1987, to December 31, 1987. The positions of the stars given in the catalog are those at the mean epoch of observations. The coordinates of the catalog are referred to the equinox and equator of J2000.0, based on the FK5 system. The mean trends of the observed positions minus FK5 positions for the FK5 basics stars are constructed and compared with those of the Tokyo PMC 86 catalog. The part I of the catalog contains the positions of 1017 FK5 basics (=FK4 stars ), 533 FK4 Suppl. stars, 2421 AGK3R stars, 1167 OB stars, 113 NPZT stars, and 84 SAO stars, and the part II of the catalog contains the positions of 413 SAO stars for occultation studies. These two parts were merged into a single pmc87 file.
The Tokyo PMC87 Catalogue, Parts I and II N sequence number in the Catalog --- Cat other catalogue name --- otherN star number in other catalogues --- otherMag visual magnitude in other catalogues mag Sp spectral type --- Epoch mean epoch of the observations of R.A. and Dec a Nobs number of observations of R.A. and Dec. --- RAh observed J2000 R.A. at the mean epoch (hours) h RAm observed R.A. at the mean epoch (minutes) min RAs observed R.A. at the mean epoch (seconds) s DE- observed J2000 Dec. at the mean epoch (sign) --- DEd observed Dec. at the mean epoch (degrees) deg DEm observed Dec. at the mean epoch (minutes) arcmin DEs observed Dec. at the mean epoch (seconds) arcsec O-C_RA (O-C) in R.A. at the mean epoch to be added to the Source Catalogue s O-C_DE (O-C) in Dec. at the mean epoch to be added to the Source Catalogue arcsec e_RAs mean error of the observed R.A. s e_DEs mean error of the observed Dec. arcsec EpMag mean epoch of the observations of magnitude a o_Mag number of observations of magnitude --- Mag observed magnitude at the mean epoch mag e_Mag mean error of the observed magnitude mag DM BD or CD numbers taken from PPM Catalog --- AGK AGK3 numbers --- CDS 1996 Feb 20 UNKNOWN UNKNOWN * 30-Sep-1991: the catalogue was supplied to CDS by Shiro Nishimura; the reformatting of the data were carried out at the Astronomical Data Analysis Center of the National Astronomical Observatory, Japan. * 20-Feb-1996: Documentation standardized, using the same description as catalog I/198 by S.Nishimura [ADAC/NAOJ], from 01-Sept-1993 I_187.xml The Tokyo PMC Catalog 88: Catalog of positions of 3800 stars observed in 1988 and planetary positions observed in 1986 to 1988 with Tokyo Photoelectric MEridian circle (PMC88) 1188 I/188 Tokyo Photoelectric Meridian Circle Catalog 1988 The Tokyo PMC Catalog 88: Catalog of positions of 3800 stars observed in 1988 and planetary positions observed in 1986 to 1988 with Tokyo Photoelectric MEridian circle (PMC88) M Yoshizawa S Suzuki M Soma Publ. National Astron. Obs. Japan 2 475 1992 1992PNAOJ...2..475Y I/186 : Tokyo PMC Catalog 85 (Yoshizawa+ 1987) I/167 : Tokyo PMC Catalog 86 (Yoshizawa+ 1989) I/187 : Tokyo PMC Catalog 87 (Yoshizawa+ 1991) I/198 : Tokyo PMC Catalog 89 (Yoshizawa+ 1993) Meridian observations Positional data The fourth annual catalog of the Tokyo PMC is presented for 3800 stars (Part I and Part II) which had been observed at least two times in the 1988 period, that is, from January 1, 1988, to December 31, 1988. The positions of the stars given in the catalog are those at the mean epoch of observations. The coordinates of the catalog are based on the FK5 system, and are referred to the equinox and equator of J2000.0. The positions of five major and nine minor planets are also given in the present catalog (Part III) for all individual observations made in 1986 to 1988. The planetary positions are based on the same coordinate systems as those of the corresponding annual star catalogs, the Tokyo PMC Catalogs 86, 87, and 88. The mean trends of the observed positions - FK5 positions for the basic FK5 stars are constructed and compared with those of the Tokyo PMC Catalogs 86 and 87. As for the planets, their observed positions are compared with the positions of the JPL's planetary ephemeris DE200. We find that the ephemerides of the outermost planets, Uranus and Neptune, have some systematic deviations of a few tenths of arcsec in longitudes.
The PMC88 Catalogue, Parts I and II N sequence number in the Catalog --- Cat other catalogue name --- otherN star number in other catalogues --- otherMag visual magnitude in other catalogues mag Sp spectral type --- Epoch mean epoch of the observations of R.A. and Dec a Nobs number of observations of R.A. and Dec. --- RAh observed J2000 R.A. at the mean epoch (hours) h RAm observed R.A. at the mean epoch (minutes) min RAs observed R.A. at the mean epoch (seconds) s DE- observed J2000 Dec. at the mean epoch (sign) --- DEd observed Dec. at the mean epoch (degrees) deg DEm observed Dec. at the mean epoch (minutes) arcmin DEs observed Dec. at the mean epoch (seconds) arcsec O-C_RA (O-C) in R.A. at the mean epoch to be added to the Source Catalogue s O-C_DE (O-C) in Dec. at the mean epoch to be added to the Source Catalogue arcsec e_RAs mean error of the observed R.A. s e_DEs mean error of the observed Dec. arcsec EpMag mean epoch of the observations of magnitude a o_Mag number of observations of magnitude --- Mag observed magnitude at the mean epoch mag e_Mag mean error of the observed magnitude mag DM BD or CD numbers taken from PPM Catalog --- AGK AGK3 numbers --- The PMC88 Catalogue, Part III Planet Name of the Planet --- Seq Sequential Number of the Observation for Each Planet --- ObsDate Julian Date of the Observation in UT1 d ObsYear Year of the observation Date --- ObsMon Month of the Observation Date --- ObsDay Day of the Observation Date --- RAh Observed Geocentric Apparent R.A. (hours) (eq=J2000) h RAm Observed Geocentric Apparent R.A. (minutes) min RAs Observed Geocentric Apparent R.A. (seconds) s O-C_RAs (O-C) in R.A. s RAcor Applied Phase Correction in R.A. s DE- Observed Geocentric Apparent Dec. (sign) --- DEd Observed Geocentric Apparent Dec. (degrees) deg DEm Observed Geocentric Apparent Dec. (minutes) arcmin DEs Observed Geocentric Apparent Dec. (seconds) arcsec O-C_DEs (O-C) of Declination arcsec DEcor Applied Phase Correction in Declination arcsec Mag Observed Magnitude mag O-C_Mag (O-C) of Magnitude mag CDS 1996 Feb 20 UNKNOWN UNKNOWN * 30-Sep-1991: the catalogue was supplied to CDS by Shiro Nishimura; the reformatting of the data were carried out at the Astronomical Data Analysis Center of the National Astronomical Observatory, Japan. * 20-Feb-1996: Documentation standardized, using the same description as catalog I/198 by S.Nishimura [ADAC/NAOJ], from 01-Sept-1993, for the pmc88 part. I_188.xml Catalogue of Positions and Proper Motions - South 1193 I/193 Positions and Proper Motions - South Catalogue of Positions and Proper Motions - South U Bastian S Roeser Astronomisches Rechen-Institut, Heidelberg ??? ??? 1993 1993pscs.book.....R Positional data Proper motions PPM South gives positions and proper motions of 197179 stars south of about -2.5 degrees declination. Its main purpose is to provide a convenient, dense and accurate net of astrometric reference stars on the southern celestial hemisphere. This net is designed to represent as closely as possible the new IAU (1976) coordinate system on the sky, as defined by the FK5 star catalogue (Fricke et al., 1988). In other words, it is a representation of this system at higher star densities and fainter magnitudes. PPM South is the southern-hemisphere complement to the PPM Star Catalogue (Roeser and Bastian, 1991), which covers the northern hemisphere, plus a strip between the equator and about -2.5 degrees declination. At the border line a continuous transition between the northern and southern part was tailored in such a way that no overlap, nor gaps, nor double entries occurred. The PPM South consists of three files: a descriptive document supplied by the authors for more detail regarding the scope, construction, properties, and usage of PPM South; the data file for the PPM South itself; and a version of PPM South for equinox and epoch B1950.0, FK4 system, in the format of the preliminary PPM North (Roeser and Bastian, 1991: Astronomisches Rechen-Institut, Heidelberg, Vols. I and II, printed by Spektrum Akademischer Verlag, Heidelberg). See the author-supplied documentation for more complete information.
Positions and Proper Motions - South PPM Designation of the star Designation of the star in PPM South starting with No. 181732, see chapter 3 of the author's description file. --- DM BD (zones -02 to -22), else CD Designation of the star in the Bonner Durchmusterung (for zones from -02 to -22 degrees) or in the Cordoba Durchmusterung (zones -23 to -89 degrees). --- mag Magnitude See chapter 3 of description file. mag Sp Spectral type --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec pmRA Proper motion in RA, J2000 Proper motion in right ascension fro epoch and equinox J2000.0, on the system of FK5 given in seconds of time per Julian year. s/yr pmDE Proper motion in DE, J2000 arcsec/yr N Number of individual published positions used Number of individual published positions used for the derivation of the position and proper motion given. --- e_RA Mean error of RA Mean error of right ascension at the mean epoch of right ascension, multiplied by the cosine of declination, given in units of #0.01 seconds of arc. 10mas e_DE Mean error of DE Mean error of declination at the mean epoch of declination, given in units of #0.01 seconds of arc. 10mas e_pmRA Mean error of pmRA Mean error of the proper motion in right ascension, multiplied by the cosine of declination, given in units of 0.001 seconds of arc per Julian year. mas/yr e_pmDE Mean error of pmDE mean error of the proper motion in declination given in units of 0.001 seconds of arc per Julian year mas/yr EpRA Weighted mean epoch, RA and pmRA Weighted mean epoch of the measured positions used for the derivation of RA and pmRA, given in years since 1900.0. yr EpDE Weighted mean epoch, DE and pmDE Weighted mean epoch of the measured positions used for the derivation of DE and pmDE, given in years since 1900.0. yr SAO SAO Designation --- HD Henry Draper Designation --- CPD Cape Photographic Durchmusterung Designation --- Flag1 'P' - problem, 'C' - comment P - problem case, preferably not to be used as astrometric reference star. C - a critical comment is given in the List of Critical Comments. Not to be used as astrometric reference star. --- Flag2 'D' - double star D - double star, preferably not to be used as astrometric reference star. --- Flag3 - not used Not used, void for consistency with PPM (north). --- Flag4 'F' - member of FK5 F - member of FK5, mostly bright stars, original FK5 data are given. --- Flag5 'R' - remark, 'V' - V mag (CPC-2) R - a remark is given in the List of Remarks on Individual Stars. V - the magnitude is a photographic V magnitude copied from CPC-2. --- PPM South - in format of old PPM North cat Characters 'PPM' --- PPM Designation of the star --- mag Magnitude mag Sp Spectral type --- Flag1 Problem flag P - problem case, preferably not to be used as astrometric reference star. C - a critical comment is given in the List of Critical Comments. Not to be used as astrometric reference star. --- RA1950 RA equinox and epoch B1950, FK4 rad DE1950 DE equinox and epoch B1950, FK4 rad pmRA1950 Proper motion in RA, B1950, FK4 0.01rad/yr pmDE1950 Proper motion in DE, B1950, FK4 0.01rad/yr RA RA equinox and epoch J2000, FK5 rad DE DE equinox and epoch J2000, FK5 rad pmRA Proper motion in RA, J2000, FK5 0.01rad/yr pmDE Proper motion in DE, J2000, FK5 0.01rad/yr descrip.doc Authors' description Lee E. Brotzman Hughes STX Gail L. Schneider NSSDC/ADC 1994 Nov 14 I_193.xml FOCAT-S: Pulkovo photographic Catalogue of Southern Hemisphere (Version 1993 March) 1195 I/195 FOCAT-S Catalogue FOCAT-S: Pulkovo photographic Catalogue of Southern Hemisphere (Version 1993 March) N F Bystrov D D Polojentsev H I Potter L I Yagudin R F Zalles J A Zelaya Bull. Inf. CDS 44 3 1994 1994BICDS..44....3B I/131A : SAO Catalogue I/146 : PPM (North) Catalogue I/193 : PPM (South) Catalogue Photographic catalog Positional data Proper motions This is a new reduction of FOCAT-S photographic catalogue of southern stars. This reduction has to replace the preceding one. The differences from previous version are as follows: 1. The new version was sorted according right ascension of stars inside 10-degree declination zone; 2. New proper motions were calculated for all almost stars. New Astrographic Catalogue plate reduction was developed for this aim. The average rms of new FOCAT-S proper motions is 0.002 - 0.003 "/year; 3. The number of the Astrographic Catalogue star positions used for the proper motion calculation is added; 4. The magnitude (mag) and spectral type (Sp) columns were revised significantly: some errors were corrected; stars identified in C.S.I. catalogue have got Mag, Sp from this catalogue as it was in previous version. Other stars have got Mag, Sp from PPM-S catalogue. 5. The list of Durchmusterung star numbers was changed. Now it contains the Cape Photographic Durchmusterung (CPD) numbers for stars in [-90, -23] declination zones; Cordoba Durchmusterung (CoD) star numbers are used only if it was impossible to identify star in BD or CPD. Format of this column was changed also. 6. PPM catalogue star numbers were added.
The FOCAT-S catalogue FOCAT-S FOCAT-S number. --- RAh Right ascension (hours) J2000. h RAm Right ascension (minutes) J2000. min RAms Right ascension (milliseconds) J2000. ms DE- Declination J2000 (sign). --- DEd Declination J2000 (degrees). deg DEm Declination J2000 (minutes). arcmin DEcs Declination J2000 (1/100 seconds). 10mas EpRA-1980 Mean epoch of right ascension, given in 0.001 of year since 1980. 0.001a EpDE-1980 Mean epoch of declination, given in 0.001 of year since 1980. 0.001a e_RA Mean error of right ascension, multiplied by the cosine of declination, in 0.01arcsec 10mas e_DEcs Mean error of declination, in 0.01arcseconds. 10mas o_RA Number of individual observations used for the derivation of the right ascension. --- o_DE Number of individual observations used for the derivation of the declination. --- n_pm proper motion flag number=1 the flag has the possible values: " " : final proper motions, derived by the new Astrographic Catalogue plate reduction; "C" : preliminary proper motions, derived using CPC2 catalogue "P" : proper motions are taken from PPM catalogue "S" : proper motions are taken from SAO catalogue "*" : proper motions are unknown. --- pmRA Proper motion in right ascension for the equinox J2000, on the FK5 system, multiplied by the cosine of declination, given in 0.001 arcseconds per Julian year. mas/a pmDE Proper motion in declination for the equinox J2000, on the FK5 system, given in 0.001 arcseconds per Julian year. mas/a e_pmRA Mean error of the proper motion in right ascension, multiplied by cosine of declination given in 0.001 arcseconds per Julian year mas/a e_pmDE Mean error of the proper motion in declination given in 0.001 arcseconds per Julian year. mas/a o_pmRA Number of individual Astrographic Catalogue observations, used for the right ascension proper motion derivation. --- o_pmDE Number of individual Astrographic Catalogue observations, used for the declination proper motion derivation. --- SpType Spectral type. --- Mag Magnitude. 0.1mag magspFlag Mag, Sp flag number=2 The flags on magnitude and spectral type indicate: " " : Mag, Sp are taken from C.S.I. catalogue "P" : Mag, Sp are taken from PPM catalogue "F" : Mag, Sp are taken from FOCAT-S source list. --- DM Durchmusterung designation number=3 The Durchmusterung designation is made of => Durchmusterung zone and star number (A8) => Durchmusterung star component (A1) => Durchmusterung designation (A1), as: "B" : Bonner Durchmusterung star number "P" - Cape Photographic Durchmusterung star number "C" - Cordoba Durchmusterung star number. --- SAO SAO catalogue star number. --- PPM PPM Catalogue star number. --- Francois Ochsenbein CDS 1995 Nov 02 We sincerely thank the Pulkovo Observatory staff for providing a tape copy. UNKNOWN UNKNOWN * Version 22-Oct-1993: from tape copy provided by the Pulkovo Observatory staff to CDS * Version 14-Apr-1994: a few errors and inconsistencies reported by S. Nishimura (NAO Japan) corrected in this Intro file at CDS * Version 02-Nov-1995: 'ReadMe' file adapted to documentation standards. I_195.xml Hipparcos Input Catalogue, Version 2 1196 I/196 Hipparcos Input Catalogue, Version 2 Hipparcos Input Catalogue, Version 2 C Turon D Egret A Gomez M Grenon H Jahreiss Y Requieme A N Argue A Bec-Borsenberger J Dommanget M -O Mennessier F Arenou M Chareton F Crifo J C Mermilliod D Morin B Nicolet O Nys L Prevot M Rousseau M A C Perryman Bull. Inf. CDS 43 5 1993 1993BICDS..43....5T I/211 : Components of Double and Multiple stars (Dommanget and Nys, 1994) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997), the resulting catalogues of the Hipparcos mission. Positional data Proper motions Photometry The Hipparcos Input Catalogue was constructed as the observing program for ESA's Hipparcos astrometry mission. This has resulted in a catalogue of stellar data including up-to-date information on positions, proper motions, magnitudes, colors, and when available, spectral types, radial velocities, multiplicity and variability information. The catalogue is complete to well-defined magnitude limits, and includes a substantial sampling of the most important stellar categories present in the solar neighbourhood beyond these limits. The magnitude limits vary from 7.3 to 9 magnitudes as a function of galactic latitude and spectral type, and there are no stars fainter than about V = 13 mag. 118000 stars are included in the Hipparcos Input Catalogue, about half of them have been selected within well-defined limits in V magnitude, spectral type and galactic latitude (the "survey"), half of them within proposed observing programs. The mean accuracies achieved, as demonstrated by comparison with the Hipparcos results (Turon et al. 1995A&A...304...82T) are 0.3 arcsec for the positions and 0.25 mag for the Hp magnitude, with accuracies of 0.02 mag or better for more than a third of the catalogue. The data set consists of the main catalogue, and the first supplement which contains more detailed information for multiple system components. Other supplements with identification charts can be found in the published version. A complete description is provided, either as a LaTeX file (intro.tex), or as a plain ascii file (intro.cat).
Hipparcos
Main Catalogue HIC Hipparcos Input Catalogue running number. --- Comp Component(s) considered in this entry --- Target Satellite target in case of joint entry Satellite target in case of joint entry (i.e.,multiple systems) : the brighter component (designated by the corresponding letter) j : the photocenter g : the geometric center (i.e., the midpoint between two components) --- RAh Right ascension J2000 (hours), at Epoch h RAm Right ascension (minutes) min RAs Right ascension (seconds) s DE- Declination J2000 (sign) --- DEd Declination (degrees) deg DEm Declination (minutes) arcmin DEs Declination (seconds) arcsec Epoch Epoch for the position, generally 2000 The Epoch for the position (years) is J2000 unless only a single epoch position is available. a e_RAs Mean error of the right ascension Mean error (in arcsec) of the right ascension value was multiplied by a factor 15.cos(delta) where delta is the declination, i.e., e_RA = 15.cos(delta)*m.e.(seconds) arcsec e_DEs Mean error of the declination arcsec r_RAs Source of position code (see Table B1) Source of positions and proper motions B : General Catalogue (Boss) C : Cape Photographic Catalogue for 1950.0 D : Catalogue of Components of Double and Multiple Stars (*) F : FK5 and FK5 extension G : Guide Star Catalog K : FK4 Supplement M : Bordeaux and/or Carlsberg automatic meridian circles N : New plate measurements or new proper motions P : Catalogue of Positions and Proper Motions (*) R : International Reference Stars (AGK3RN, SRS (*)) S : Smithsonian Astrophysical Observatory Star Catalogue T : Cape Catalogue of Faint Stars X : Miscellaneous Y : Sydney Southern Star Catalogue 2 : Second Cape Photographic Catalogue 3 : Catalogue of Standard Stars Based on the N30 System 5 : Second Cape Photographic Catalogue for 1950.0 (*) preliminary version For further details, see Table B1 of the full documentation. --- RAdeg Right ascension J2000 (decimal degrees) deg DEdeg Declination J2000 (decimal degrees) deg GLON Galactic longitude (decimal degs) deg GLAT Galactic latitude (decimal degrees) deg ELON Ecliptic longitude (decimal deg) deg ELAT Ecliptic latitude (decimal degrees) deg RAh1950 Right ascension B1950, epoch=1950.0 unless Epoch differs from 2000 (hours) h RAm1950 Right ascension (minutes) min RAs1950 Right ascension (seconds) s DE-1950 Declination sign, B1950 --- DEd1950 Declination (degrees) deg DEm1950 Declination (minutes) arcmin DEs1950 Declination (seconds) arcsec RAdeg1950 Right ascension B1950 (decimal degrees) deg DEdeg1950 Declination B1950 (decimal degrees) deg pmRA Proper motion in RA, Equinox J2000.0 The proper motion mu_alpha in RA is in arcsec per year. The Equinox is J2000.0. The value in the table is 15.mu_alpha*cos(delta). arcsec/a pmDE Proper motion in dec, Equinox J2000.0 arcsec/a e_pmRA Error of pmRA arcsec/a e_pmDE Error of pmDE arcsec/a r_pmRA Source of proper motion (see Table B1) --- Hp Magnitude in the Hipparcos photometric system. mag Var Variability code (range 1-5; see Table V1) The variability code provides information on known or suspected variable stars (all amplitudes are in Hp): (blank): the star is not a known or suspected 1 : suspected variable, with a suspected amplitude variation smaller than 2 mag 2 : suspected variable, with a suspected amplitude variation larger than 2 mag 3 : known variable, with an amplitude variation larger than 0.2 mag 4 : known variable, with large amplitude (> 2 mag), for which an ephemeris was necessary 5 : known variable, with an amplitude variation smaller than 0.2 mag --- Std Standard star code Standard code: C : Photoelectric standard star with confirmed long-term stability S : Secondary photoelectric standard star. --- Vmag V magnitude mag e_Vmag Error of V magnitude mag B-V B-V colour index mag e_B-V Error of B-V mag r_B-V Source of photometry (see Table B2) Source of photometry A : Photographic B or V from SIMBAD or proposers; colour from spectral type C : V magnitude derived from CAMC; colour from spectral type D : Joint systems with combined or joint magnitude and colour P : Photoelectric photometry V : Variable stars (amplitude larger than 0.2 mag) X : Miscellaneous For further details, see Table B2 of the full documentation. --- Sp Spectral type and luminosity class The spectral type and luminosity class are from various sources and follow various classification schemes. The following signs are also used: : indicates some doubt about the given values /,- between two spectral types or luminosity classes: / indicates Survey - indicates that the parameter is intermediate between those given +... indicates composite spectra ... indicates truncated spectra (see the source catalogue for more details, such as peculiarities) --- r_Sp Source of the spectral type (see Table B3) Source of Spectral Type and Luminosity Class 1 : Michigan Spectral Survey, Vol. 1 2 : Michigan Spectral Survey, Vol. 2 3 : Michigan Spectral Survey, Vol. 3 4 : Michigan Spectral Survey, Vol. 4 K : Fourth Edition of GCVS S : SIMBAD X : Miscellaneous For further details, see Table B3 of the full documentation. --- Plx Parallax (milli-arcsec) mas e_Plx Probable error of parallax (milli-arcsec) mas n_Plx Type of parallax Type of parallax: T : trigonometric D : dynamical --- RV Radial velocity km/s q_RV Quality of RV, a=best Quality of Radial Velocity (based on the number of observation, spectrograph dispersion, and interagreement of separate determinations) a : 0.5 km/s b : 1.3 km/s c : 2.5 km/s d : 5 km/s e : not given --- r_RV Source of RV (see Table B4) Source of Radial Velocity B : Barbier-Brossat (1989) E : Evans (1978) W : GCRV (Wilson 1953) X : Miscellaneous For further details, see Table B4 of the full documentation. --- Vname Variable star name (GCVS or NSV) --- VarType Type of variability (see Table V2) For further details, see Table V2 of the full documentation. --- Period Period of variation (days) d Vmax V magnitude at maximum luminosity. mag Vmin V magnitude at minimum luminosity. mag q_Vmax Coded error of Vmax and Vmin, 1=best This code gives an estimation of the accuracy of the V magnitudes at maximum and minimum luminosity given in fields 42 and 43. This estimate includes the errors of individual measurements and the possible variability of the maxima and minima. This information is given for stars with a variability code of 3 or 4 (as specified by the first char of field 26), whenever the necessary information on the luminosity curve was available. The code can take the following values: 1 : <= 0.2 mag 2 : 0.2 - 0.5 mag 3 : 0.5 - 1.0 mag 4 : >= 1.0 mag --- MagCode Code specifying magnitudes and colour Code specifying the magnitudes and colour given in fields Hp, V, and B-V. This information is given for stars with a variability code of 3 or 4 (as specified by the first character of field 26), whenever the necessary information on the luminosity curve was available. 1 : magnitude at minimum luminosity 2 : magnitude at maximum luminosity 3 : mean magnitude 4 : weighted magnitude (0.33 max + 0.67 min) for most pulsating stars 5 : weighted magnitude (0.85 max + 0.15 min) for eclipsing systems --- CCDM CCDM number (details in annex1) Provisional version of the Catalogue of the Components of Doubles and Multiple Stars (See <I/211>) --- CCDMcomp Components considered --- PA Position angle components Position angle between components considered is defined with the origin at the North and increasing through increasing right ascension. For some stars only a rough indication of the position angle is given and not a value in degrees: 'F' : following, 'P' : preceding, 'N' : North, 'S' : South, or a combination of these letters. deg Sep Separation between the components considered. arcsec Dmag Magnitude difference between the components mag n_CCDM Information on orbital systems O : system with know orbit A : system is a known astrometric binary * : the astrometric binary is also a member of an orbital system --- BD BD number. Last char: suffix to BD --- CD CD number. --- CPD CPD number. --- HD HD/HDE number. --- FK FK5/FK5 Ext/FK4 Sup or IRS (AGK3R/SRS) number The FK5, FK5 Extension, FK4 Supplement, or IRS (which comprises the AGK3R/SRS) number are given. ------------------------------------------------------ Catalogue Format Range No. Stars ------------------------------------------------------ A : AGK3R NNNNN 1-21499 19777 F : FK5 NNNN 1- 1670 1535 F : FK5 Ext NNNN 2001- 6125 3103 K : FK4 Sup NNNN 2001- 3997 995 S : SRS NNNNN 1-20495 15472 --- AG AGK3/CPC number (see Table I2) The AGK3 and CPC number are given. ------------------------ AGK3 +/- DD NNNN CPC VV NNNNN or VV.v NNNNN Other(*) 0 NNNNN ------------------------ (*) given in the zone -52 to -40deg, following the system adopted within SIMBAD, with cross-identifications made with the Cape Zone Catalogue. For further details, see Table I2 of the full documentation. --- SAO SAO number --- Ident1 First of two selected identifiers Up to two identifiers are given in these two fields: GL, GJ, G, LHS, LTT, LP, L, BPM, CF, McC ( according to this hierarchy). For further details, see Table I3 of the full documentation. --- Ident2 Second of the two selected identifiers --- Ident3 Other identifiers Identifier for stars in: - galactic open clusters (see Table B5) - Large and Small Magellanic Clouds Sk : Large Magellanic Cloud (Sanduleak, 1969a) -DD NNN Sk : Small Magellanic Cloud (Sanduleak, 1968, 1969b) NNN For further details, see Table I4 of the full documentation. - Stars in following catalogues: C* : Cool Carbon Stars (Stephensen, 1973) IRC : Caltech 2 micron Survey (Neugebauer et al. 1969) PK : Planetary Nebulae (Perek and Kohoutek, 1967) WD : White Dwarfs (McCook and Sion, 1977) For further details, see Table I5 of the full documentation. --- Status Miscellaneous information S : Survey star C : Identification chart provided within the faint star Atlas (annex 2 of the printed version) T = S+C --- Notes additional notes, detailed in file "notes" N : Note explained in the "notes" section of the accompanying full documentation (section 17), and also in file "notes". --- Double and Multiple System Components CCDM CCDM number (Catalogue <I/211>) --- rComp Reference component when different from A --- Comp Component considered --- HIC HIC number as in 'main' file --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Mag Magnitude (generally V, sometimes photographic for the faintest systems) mag Obs Year of observation of the relative position a PA Position angle deg Sep Separation (arcsec) arcsec Note1 O=system with known orbit --- Note2 A=astrometric binary --- pmRA Proper motion in right ascension =15.mu_alpha*cos(delta) arcsec/a pmDE Proper motion in declination arcsec/a DM DM number. Last char is a suffix to DM, or "*" if HD convention is not followed. --- HD HD/HDE number --- AG AGK3 or SAO number --- IDS IDS number (equinox B1900), with component indication. --- ADS ADS number --- Notes to marked HIC stars. HIC Hipparcos Number --- Text Text of note --- intro.tex LaTeX description formats.tex Formats in LaTeX N. P. Kuin ADC 1995 rev. C. Turon [Meudon] 22-Oct-1996 Nov 04 UNKNOWN UNKNOWN * Version 1 of HIC was numbered I/191, and announced in the Bull. Inf. CDS, 9 (1992) * 30-Jun-1993: original version ReadMe file [CDS] * 08-Nov-1994: This ReadMe file rewritten by N. P. Kuin [ADC] * 23-Oct-1996: This ReadMe file revisited by C. Turon, Paris-Meudon (catherine.turon@obspm.fr) * 06-Oct-1997: Added the "notes" file (extracted from intro.cat) I_196.xml The Tycho Input Catalogue. Cross-matching the Guide Star Catalog with the Hipparcos INCA Data Base 1197A I/197A Tycho Input Catalogue, Revised version The Tycho Input Catalogue. Cross-matching the Guide Star Catalog with the Hipparcos INCA Data Base D Egret P Didelon B J McLean J L Russell C Turon Astron. Astrophys. 258 217 1992 1992A&A...258..217E I/196 : Hipparcos Input Catalogue, Version 2 (Turon+, 1993) I/207 : Preliminary list from Tycho observations (Halbwachs+ 1994) Positional data Photometry A Tycho Input Catalogue of three million stars brighter than V=12.1 has been prepared, for the needs of the Tycho mission (Hipparcos satellite). This catalogue results from the cross-matching of a subset of the Hubble Space Telescope Guide Star Catalog with the Hipparcos INCA database. References to these major catalogues, and details about the cross-matching procedures are to be found in the paper published in Astron. Astrophys. 258, 217-222 (May 1992). Among the 3,154,204 stars of the Tycho Input Catalogue, only a bit more than 1 million will appear in the final Tycho catalogue. A preliminary selection was done in the Recognition process, that was based on the first year of the satellite scientific mission (Halbwachs et al., =1994A&A...281L..25H). 1,049,971 stars were thus selected, and are flagged in this version of the Tycho Input Catalogue.
The catalogue, zones 0/37.5deg The catalogue, Zones 37.5/90deg The catalogue, Zones 0/-37.5deg The catalogue, Zones -37.5/-90deg TICID1 GSC region number --- TICID2 GSC running number in region --- RA10mas Right ascension J2000.0 Epoch 1990, in 0.01arcsec 10mas SPD10mas South Polar Distance (=Dec+90) Epoch 1990, in 0.01arcsec 10mas e_pos Error on position in 0.01arcsec 10mas e_B Error on B mag. in 0.01 mag. (0=unknown) .01mag B B magnitude in 0.01 mag. (0=unknown) .01mag e_V Error on V mag. in 0.01 mag. (0=unknown) .01mag V V magnitude in 0.01 mag. (0=unknown) .01mag Flag1 FK5 star --- Flag2 IRS star --- Flag3 Photometric standard for Tycho --- Flag4 Monitor star : random set --- Flag5 Monitor star : selected from TIC flags --- Flag6 Monitor star : NGC, ADS system --- Flag7 Photometric star --- Flag8 Monitor star (logical OR of #1 to #6) --- Flag9 GSC/INCA discrepancy --- Flag10 Star selected in the Recognition process --- Flag11 GSC/INCA magnitude discrepancy --- Flag12 INCA (or CDA) entry NOT in GSC 1.0 --- Flag13 Source of position (0: GSC; 1: INCA) --- Flag14 id.- for B magnitude --- Flag15 id.- for V magnitude --- Flag16 Non-stellar GSC image ("unknown" class) --- Flag17 Component of TIC pair (sep. < 20") --- Flag18 Close pair with one single entry (sep < 3") --- Flag19 Component of INCA pair (sep < 10") --- Flag20 INCA/CDA star (cross-id. in Annex file) --- Flag21 Known proper-motion --- Flag22 Known high proper-motion (>0.15"/yr) --- Flag23 Known parallax --- Flag24 Known variable --- Flag25 Known multiple system --- Flag26 Hipparcos Input Catalogue star (Annex file) --- Flag27 CDA star (complementary astrometric data) --- Annex file, Cross-identifications TICID1 GSC region number --- TICID2 GSC running number in region --- NCSI CSI number (from SIMBAD and the INCA database) --- Comp Component code (A, B, AB, etc.) or blank --- ID Star Identification (from HD, DM, or other catalogues) --- Dmag Mag(GSC) - Mag(INCA) mag Dpos Distance pos(GSC)-pos(INCA) in arcsec. arcsec HIC HIPPARCOS Input Catalogue number --- N.P.M. Kuin ADC 1994 Nov 09 UNKNOWN UNKNOWN * 10-Jan-1994: Original version of this file: Jean-Louis Halbwachs [CDS] * 09-Nov-1994: This file rewritten by N.P.M. Kuin [ADC] UNKNOWN UNKNOWN Notes and warnings concerning the present release: The following corrections have been applied to the TIC, generating some differences with respect to the 'operational' version of TIC described in the Astron. & Astrophysics paper : o corrected coordinates for high proper motion stars (see footnote 2 in the A&A Paper). These stars are the stars with flag 12 (INCA star without GSC counterpart) and flag 22 (proper motion larger than 0.15"/yr). 2130 objects in TIC have both flags set. For these stars, the original INCA position (at epoch 1990) have been searched for, and the correct positions restored. o additional TIC entries have been assigned a consistent GSC number provided by the STScI team (rather than a number starting at 10001); note that the brighter ones (V< 7.5) appear in GSC version 1.1, with plate name +056. o in three GSC regions (3588, 5706, and 7899) where the numbering sequence restarts to 0 after 10000 in the GSC (in the CD-ROM edition of GSC only the last four digits are printed), correct numbers have been restored in TIC (thus in the range 10000-13000). o The HIC numbers in the annex file have been updated (from the old IC5 in the 'operational version', to the HIC numbers as published in ESA SP-1136). Note that there are 23 HIC duplicates (TIC entries having the same HIC number : these are A and B components of close systems), and that there are 110 entries which have been suppressed from the Hipparcos Catalogue after the start of the mission and before the publication of the Catalogue (see Table 1 in ESA SP-1136). o The annex file contains also 60 INCA duplicates (TIC entries having the same INCA identification); this is due to late corrections in the INCA file, and the duplicate TIC entry is likely to be redundant. I_197A.xml The Tokyo PMC Catalog 89: Catalog of Positions of 3866 Stars Observed in 1989 and with Tokyo Photoelectric Meridian Circle 1198 I/198 Tokyo Photoelectric Meridian Circle Catalog 1989 The Tokyo PMC Catalog 89: Catalog of Positions of 3866 Stars Observed in 1989 and with Tokyo Photoelectric Meridian Circle M Yoshizawa S Suzuki Publ. Nat. Astron. Obs. Japan 3 45 1993 1993PNAOJ...3...45Y I/186 : Tokyo PMC Catalog 85 (Yoshizawa+ 1987) I/167 : Tokyo PMC Catalog 86 (Yoshizawa+ 1989) I/187 : Tokyo PMC Catalog 87 (Yoshizawa+ 1991) I/188 : Tokyo PMC Catalog 88 (Yoshizawa+ 1992) I/146 : PPM North Star Catalogue (Roeser+, 1988) I/193 : PPM South Star Catalogue (Bastian+ 1993) Meridian observations Positional data The fifth annual catalog of the Tokyo PMC is presented for 3466 stars (Part I and Part II) which were observed at least two times in the 1989 period, that is, from January 1, 1989, to December 31, 1989. The positions of the stars given in the catalog are those at the mean epoch of observations. The coordinates of the catalog are based on the FK5 system, and refer to the equinox and equator of J2000.0. The values of (O-C)s in the catalog are calculated by using the positions given in the source catalog, and by evaluating those at the mean epoch of observations of each star, with the equinox and equator at the mean epoch. The magnitudes of the stars given in the catalog can be transformed into the V-magnitude of the standard UBV system by the equation: V = V(TPMC) + 0.063 ( B-V ) - 0.045. The mean trends of the observed positions-FK5 positions for the basic FK5 stars are constructed and compared with those of the Tokyo PMC Catalogs 86, 87, and 88. The Part I of the catalog contains the positions of 1080 basic FK5 stars, 210 FK4 Suppl. stars, 1700 AGK3R stars, 131 OB stars, 36 NPZT stars, and 96 SAO stars, observed with the Tokyo PMC in the 1989 period based on FK5 system. The Part II of the catalog contains the positions of 210 zodiacal stars observed with the Tokyo PMC in the 1989 period based on the FK5 system. The stars of the Part II are usable for the reduction of lunar occultation. The Parts I and II are concatenated to form a single machine-readable catalog.
The catalog (Parts I & II) N sequence number in the Catalog --- Cat other catalogue name --- otherN star number in other catalogues --- otherMag visual magnitude in other catalogues mag Sp spectral type --- Epoch mean epoch of the observations of R.A. and Dec a Nobs number of observations of R.A. and Dec. --- RAh observed J2000 R.A. at the mean epoch (hours) h RAm observed R.A. at the mean epoch (minutes) min RAs observed R.A. at the mean epoch (seconds) s DE- observed J2000 Dec. at the mean epoch (sign) --- DEd observed Dec. at the mean epoch (degrees) deg DEm observed Dec. at the mean epoch (minutes) arcmin DEs observed Dec. at the mean epoch (seconds) arcsec O-C_RA (O-C) in R.A. at the mean epoch to be added to the Source Catalogue s O-C_DE (O-C) in Dec. at the mean epoch to be added to the Source Catalogue arcsec e_RAs mean error of the observed R.A. s e_DEs mean error of the observed Dec. arcsec EpMag mean epoch of the observations of magnitude a o_Mag number of observations of magnitude --- Mag observed magnitude at the mean epoch mag e_Mag mean error of the observed magnitude mag DM BD or CD numbers taken from PPM Catalog --- AGK AGK3 numbers --- S.Nishimura ADAC/NAOJ 1993 Sep 01 I_198.xml Lick Northern Proper Motion Program: NPM1 Catalog 1199 I/199 Lick Northern Proper Motion Program: NPM1 Catalog Lick Northern Proper Motion Program: NPM1 Catalog A R Klemola R B Hanson B F Jones Astron. J. 94 501 1987 1987AJ.....94..501K Positional data Proper motions Magnitudes, photographic Colors Cross identifications The NPM1 catalog is the first part of the Lick Northern Proper Motion (NPM) program to measure absolute proper motions, on an inertial system defined by some 50,000 faint galaxies, for some 300,000 stars over a blue apparent magnitude range from 8 to 18. There are 1246 6-degree by 6-degree fields in the NPM survey (to declination -23 degrees). The NPM1 catalog covers the 72% of the northern sky lying outside the Milky Way and contains some 149,000 stars from measures in 899 of the 1246 NPM fields. A second catalog (NPM2) will cover the NPM Milky Way fields. The Yale Southern Proper Motion (SPM) program will complete the southern sky. Each NPM field was photographed at two epochs between 1947 and 1988. The mean first and second epochs are 1950 and 1977; the average epoch difference is 27 years. The first-epoch plates were taken in the blue only; both blue and yellow plates were taken at the second epoch. Some 94000 stars were chosen anonymously for the NPM astrometric reductions and for statistical studies of stellar motions. In addition, the NPM1 catalog contains some 28000 positional reference stars, and some 27000 stars were chosen from the Lick Input Catalog of Special Stars (ICSS). Positions are given for equinox B1950 and computed epoch 1950. Each star's entry includes the absolute proper motion and blue magnitude. For 97% of the stars the color is also given. Other data given for each star are: the original mean epoch, a stellar class code, the number of NPM fields measured, and discrepancy flags for position, proper motion, and photometry. Finally, as an additional identification, the AGK3 (north) or SAO (south) number (if any) is given. The rms errors of the NPM absolute proper motions are about 0.5"/cent in each coordinate. The rms position errors at the catalog epoch 1950 average about 0.15" in each coordinate. The rms errors for the NPM photographic photometry average about 0.2 mag in B, and 0.15 mag in B-V. More complete descriptive information is available in the ASCII or LaTeX documentation written by A.R. Klemola, R.B. Hansen, and R.B. Jones (UCO/Lick Obs.)
The Catalogue Name NPM1 star "name" made of: Byte 1 : Sign of declination for this zone Bytes 2-3: Declination zone Bytes 4-8: Running number in this declination zone --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec pmRA Absolute proper motion RA (in "/century) arcsec/hyr pmDE Absolute proper motion Dec. arcsec/hyr B Photographic photometry (B magnitude) mag B-V =-9.99 Photographic photometry (B - V color) (= -9.99 if no data) mag Epoch Original mean epoch of position (-1900) yr class Code for class of star The code is a sum of the following numbers, if applicable. +1 if anonymous star (faint or bright) +2 if catalog star (AGK3 or SAO) +4 if other star (Lick Input Catalog) --- nfields Number of NPM fields on which star was measured --- ips Discrepancy flag Position As defined in Table 2 of the Document file (npm1.txt) ---------------------------------------------------- Position Proper Motion Photometry ---------------------------------------------------- Flag=0 O.K. O.K. O.K. Flag=1 R.A. R.A. B Flag=2 Dec. Dec. B - V Flag=3 Both Both Both Flag=9 Error Error Error ---------------------------------------------------- Limits 1.0 arcsec 3.0 arcsec/cent 1.0 mag --- ipm Discrepancy flag Proper Motion --- ibv Discrepancy flag Photometry --- icatno AGK3 and SAO identification AGK3 identification for zones +89 to -01 SAO identification for zones -02 to -23 --- agksgn AGK catalog identification blank if AGK zone = NPM zone + if AGK zone = NPM zone + 1 - if AGK zone = NPM zone - 1 --- npm1.txt ASCII Catalog Description npm1.tex LaTeX Catalog Description N. Paul M. Kuin and Gail L Schneider NSSDC/ADC 1994 Nov 22 I_199.xml Lick Northern Proper Motion Program: NPM1 Reference Galaxies 1200 I/200 Lick Northern Proper Motion Pgm: NPM1 Ref Gal Lick Northern Proper Motion Program: NPM1 Reference Galaxies A R Klemola R B Hanson B F Jones Astron. J. 94 501 1987 1987AJ.....94..501K Galaxy catalogs Positional data Magnitudes, photographic The Lick Northern Proper Motion (NPM) program measured proper motions, positions, and photographic photometry for some 149,000 stars (NPM1 Catalog) covering the sky outside the Milky Way north of declination 23 degrees. The NPM1 proper motions were measured with respect to an absolute reference frame defined by some 50,000 faint galaxies (mostly 16 < B < 18 mag). The rms position errors for the NPM1 reference galaxies average 0.2 arcsec. The rms errors for the B magnitudes average 0.25 mag. More complete descriptive information is available in the ASCII or LaTeX documentation written by R.B. Hansen (UCO/Lick Obs.).
The Catalogue Name NPM1 galaxy "name": Byte 1 : Sign of declination for this zone Bytes 2-3: Declination zone Bytes 4-8: Running number in this declination zone --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec bmag Photographic photometry (B magnitude) mag nfields Number of NPM fields on which this galaxy was measured --- ips Discrepancy flag Position defined in Table 2 of the Document file (npm1.txt) ---------------------------------------------------- Position Proper Motion Photometry ---------------------------------------------------- Flag=0 O.K. O.K. O.K. Flag=1 R.A. R.A. B Flag=2 Dec. Dec. B - V Flag=3 Both Both Both Flag=9 Error Error Error ---------------------------------------------------- Limits 1.0 arcsec 3.0 arcsec/cent 1.0 mag --- ipm Discrepancy flag Proper Motion --- ibv Discrepancy flag Photometry --- npm1rgal.txt ASCII Catalog Description npm1rgal.tex LaTeX Catalog Description N. Paul M. Kuin and Gail L. Schneider NSSDC/ADC 1994 Nov 09 I_200.xml XZ Catalog of Zodiacal Stars 1201 I/201 XZ Catalog of Zodiacal Stars XZ Catalog of Zodiacal Stars D W Dunham W H Warren Jr. unpublished ??? ??? 1995 1995 Astrometric data Combined data Positional data Zodiacal regions The XZ catalog was created at the U. S. Naval Observatory in 1977 by Richard Schmidt and Tom Van Flandern, primarily for the purpose of generating predictions of lunar occultations, and for analyzing timings of these events. It was designed to include all stars from Robertson's Zodiacal Catalog (ZC), the SAO catalog, and the AGK3 catalog that are within 6d 40' of the ecliptic, which is as far as the Moon's limb can ever get as seen from anywhere on the Earth's surface, leaving some margin for stellar proper motions and change in the obliquity of the ecliptic over the course of three centuries. The original version contained 32,221 entries. Since that time, a number of changes have been made in suceeding versions, including better positions and proper motions, and the elimination and addition of stars. The catalog contains visual magnitudes and radial velocities as well as astrometric data.
The XZ catalog was created at the U. S. Naval Observatory in 1977 by Richard Schmidt and Tom Van Flandern, primarily for the purpose of generating predictions of lunar occultations, and for analyzing timings of these events. It was designed to include all stars from Robertson's Zodiacal Catalog (ZC), the SAO catalog, and the AGK3 catalog that are within 6d 40' of the ecliptic, which is as far as the Moon's limb can ever get as seen from anywhere on the Earth's surface, leaving some margin for stellar proper motions and change in the obliquity of the ecliptic over the course of three centuries. Hereafter, this region will be called "the Zodiac". The catalog contains 32,221 entries. Two years after the catalog was created, and observations were already reported using its numbers, it was found that about 200 stars near the equator from the AGK3 catalog were outside the Zodiac, and a similar number that should have been included were not. Since the numbering system had already been established, the catalog was not changed to correct this deficiency. Over the years, some errors in the catalog, due mainly to errors in the SAO and AGK3, were corrected. A few stars with very bad data were "eliminated" by changing their declination to -89d and adding 40 to their magnitudes. In 1986, most of the stellar positional data were replaced with improved data from Harrington's and Douglass' Zodical Zone (ZZ) catalog, which used for its observing list SAO stars in the Zodiac (actually broader than the XZ Zodiac because ecliptic latitudes to +/-15d were used) north of declination approximately -25d. The positional data for many of the stars south of declination -25d with right ascensions greater than 18h were improved with data from the Lick Voyager Uranus catalog. In 1991, the photographic magnitudes of the AGK3 stars not in the SAO were converted to photovisual magnitudes by applying corrections based on each star's spectral type, when available. Stellar magnitudes and double-star codes have been updated periodically based on reports from observers. Each time a series of updates was made, the XZ version was changed. The current version is XZ80N, created during the summer of 1992. Late in the summer of 1992, Mitsuru Soma in Japan created a J2000 version of the XZ, which we call XZ80NJ2. The next update is planned for 1994, when the positional data may also be replaced with PPM data; probably only the J2000 version will be updated. The XZ catalog is no longer maintained at the U. S. Naval Observatory (USNO); it is now maintained by the International Occultation Timing Association (IOTA). The changes made to the different versions of the XZ catalog during the past several years have been documented in Occultation Newsletter, IOTA's quarterly publication.
B1950.0 catalog J2000.0 catalog X --- num Sequential number --- dmID Durchmusterung identifier --- dmsign Sign of DM zone --- dmzone Durchmusterung zone --- dmnum Durchmusterung number --- dscode Double-star code Listed below are the double-star codes currently in use. For "triple," three stars are usually meant, but there may be other known stars in the system. A - Listed by Aitken and/or Burnham (ADS, BDS) B - Close double with third star nearby with separate XZ number C - Listed by Innes, Couteau, or other visual observers D - Primary of double; secondary has separate XZ entry E - Secondary of double; primary has separate XZ entry F - Following component G - A or C with second star either M, J, U, or V and third star referred to second star H - Triple: J, U or V and M I - O with secondary either J, U, or V (third star's data referred to secondary) J - Single-lined spectroscopic binary; separation probably <0.01" K - U or V, but duplicity doubtful ("possible" double) L - Triple: J or U, and V; or all V; or all J M - Mean position of close pair N - North component O - Orbital elements available P - Preceding component Q - Triple: J or U or V, and O R - Triple: O and O S - South component T - Triple: V and A or C; or all A and/or C U - Separation <0.01" (usually 2-line spectroscopic binary) V - Separation >0.01", but not visual (occultation, interferometric, or speckle component) W - Triple: J or U, and A or C X - Probably a close double, not certain Y - Triple: K or X, and A or C Z - Triple: O and A or C or V or X or L $ - M with secondary either M, J, U, or V (third star's data referred to secondary star) --- m(v) Visual magnitude mag RAh Right ascension (B1950.0) The epoch and equinox of the Right Ascension and Declination have been B1950 for most of the history of the XZ. In 1992, Mitsuru Soma at the National Observatory in Mitaka, Japan, made a J2000 version of XZ80N, where the epoch and equinox of the R.A. and Dec. were converted to J2000 from B1950 using the Astronomisches Rechen-Institut's procedure for this conversion. h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s pmRA Proper motion in RA 0.01s/a De- Sign of declination --- DEd Declination (eq & ep B1950.0) The declinations can be read into one double-precision variable with an F9.2 format, rather than with a format such as given (separate variables for d,',""), although the sign is always in byte 39. Save the original read-in value (so it can be tested at the end for the sign), then take its absolute value for decoding into degrees, minutes, and seconds of arc. A subroutine like the Fortran function SECNDS can be used convert the full number into seconds of arc counted from the equator; it can similarly be used to convert the right ascensions into seconds of time, 0 - 86400, counted from the equinox, by reading the R.A. as one double-precision number with an F9.3 format rather than with the format indicated. deg DEm Declination (eq & ep B1950.0) arcmin DEs Declination (eq & ep B1950.0) arcsec cpmDE Proper motion in Dec 0.01arcsec/a pi Trigonometric parallax arcsec RV Radial velocity km/s cat2cd Second catalog code (*) 80 AGK3 (not ZC, not SZ; the second catalog code number in this case is the number of the star in the AGK3 zone, which can be determined from the degrees of declination for the J2000 version of the catalog; for these stars, the AGK3 zone and number are also given in the name fields) 90 ZC (Robertson ZC) 94 SZ (SAO, not ZC; the SZ was a Zodical subset of the SAO catalog, a predecessor of the XZ that was replaced by the XZ) --- cat2num Second catalog number --- SAO SAO Catalog number Some stars are not in the SAO catalog, mainly stars whose data were obtained from the AGK3. In the Zodiac, the SAO numbers are always greater than 50,000. So the SAO field was used for the AGK3 error code, which ranges from 1 to 16. If the second catalog code is80 and the SAO number is within the range of 1 to 16, the SAO number is actually an AGK3 error code. --- sp Spectral type --- eRA Error in RA (at epoch) s epmRA Error in RA PM (at epoch) s/a eDE Error in Dec (at epoch) arcsec epmDE Error in Dec PM (at epoch) arcsec epoch Epoch - 1850 (integer years) This is the mean epoch of the observations that should be used only for calculating the error in the star's position at a specified time when using the errors in bytes 80-95. yr name Star name or catalog designation The star names sometimes extend into the coding field when there is no code present. The codes give information on source catalogs and their numbers. Bytes 99-122 can just as well be read as a single field with A24. Bytes 121-122 contain a code if byte location 120 is blank; if byte location 120 is not blank, then bytes 121-122 contain the end of the star name. If one wants only the star names and not the code, byte location 120 must be tested for blank; if it is blank, then bytes 121-122 should be replaced with two blank bytes. --- code Special coding --- encode Encoding for bytes 116-120 --- source Source catalog code Source catalog codes 10-60 XZ/SAO 69 XZ/GC 70 SAO/GC (very poor data) 76 XZ/GC 80 AGK3/XZ 81 ZC/Perth 70 (combined ZC and P70 data) 82 Yale 84 Lick Voyager catalogs (usually combined with SAO data) 90 ZC/XZ 91 FK4 92 FK4 Supplement/FK3 93 N30 96 Pleiades catalog (Eichhorn) 97 ZZ87 (Harrington and Douglass) 98 Perth 70 --- xz80n.doc The original document N. G. Roman NASA/NSSDC/ADC 1995 Feb 28 UNKNOWN UNKNOWN Other USNO lunar occultation catalogs: David Dunham created other star catalogs for special occultation predictions at USNO; these have a format similar to that of the XZ, where the character in byte location 1 identified the catalog, when field 1 was included. In 1977, the K-catalog was created just before the XZ, to include AGK3 and southern Yale catalog stars (a few hundred, some as bright as 7th mag., were not in the SAO catalog, and therefore not in the SZ, since no proper motions were given for them) that were not in the SZ catalog being used at the time. It included more than 7000 stars to supplement the SZ. In 1978, after the XZ was established and used for occultation predictions, the K-catalog was modified so that it would exactly supplement the XZ, but without changing the sequence, since predictions had already been distributed and observations reported using K-catalog numbers in 1977. Most (but not all) of the AGK3 stars in the K-catalog are also in the XZ, so these were "removed" (at least for lunar occultation prediction purposes) by changing the degrees of declination of these stars in the K-catalog to -89. So although there are still more than 7000 entries in the K-catalog, only several hundred of them are valid; other users may simply want to remove the invalid entries by rejecting all stars with declinations less than -88d. The other catalogs do not cover the whole Zodiac, but only certain fields of special interest, such as galactic clusters and star fields that were traversed by the Moon during total lunar eclipses. These catalogs include stars down to 11th and 12th magnitude usually obtained from the Astrographic Catalogs. They were cross-referenced with the XZ, and the data of matched stars replaced with XZ data; the X or ZC number for such stars was given in the DM field #2, which for these catalogs must be read with the format A3,I5, since non-numeric data are sometimes included in all byte locations of the "zone". The occultation prediction program at USNO required stars to be located at every hour of right ascension. Therefore, "spacer" entries were needed for these catalogs to fill this requirement. The magnitudes of these false-star entries were given as either 40 or 50 and the declinations as either -89d or -90d. Be careful when using the declinations from these other catalogs, since, unlike the XZ, the sign of the declination is not always in byte location 37. The declinations should be read with an F9.2 format, since the minus for negative declinations is not always in byte locations 37 or 38. Save the original read-in value (so it can be tested at the end for the sign), then take its absolute value for decoding into degrees, minutes, and seconds of arc. A subroutine like the Fortran function SECNDS can be used convert the full number into seconds of arc counted from the equator; see the appendix below. The other catalogs are listed below. Logical Physical Occultation Cat. Record Record Newslet. Ref. Name Length Length Vol./No./pages Brief description ------------------------------------------------------------------------------ 5BM 80 8000 1/4/29-31 For 1975 May lunar eclipse 2/4/37 M, mainly for 1979 eclipses 3/1/3 B, for 1981 eclipses "5BM" is an RA-sorted combination of the above 3 catalogs E 86 8600 3/12/249 & For eclipses in 1985 and 1986 3/16/345 J 104 10400 1/13/138-139 Hyades, Milky Way, 1977 eclipses, & 1/14/145-147 other clusters & 1/16/170 C 104 10400 2/14/188-189 Milky Way, 1982 eclipses, clusters & 2/16/222-224 K 86 8600 1/13/138-139 See above L 86 8600 4/11/263-266 1989-90 eclipses, Lick-Voyager cats. & 4/12/301 & 4/14/336 The above describes the format of the 123-byte records in the normal export version of the XZ catalog. However, different variations on this format have been used for internal use at the U. S. Naval Observatory and for the other catalogs. They are descibed below for the different logical record lengths involved. Record Length Description ------------------------------------------------------------------------------ 80 Includes fields 2-19 described above, that is, byte locations 7 - 96. 86 Includes fields 1-19 described above, that is, byte locations 1 - 96. The first byte location contains the single-letter USNO catalog code identifier (E, K, etc.). 104 Includes fields 2-21 described above, that is, byte locations 7 - 119. The C and J catalogs use this format, and some of the records at the end of the catalog (at least for C) are blank. For the C and J catalogs, the name fields (20 and 21) are all blank. Since the 80- and 104-byte versions do not include field 1 (XZ number), the sequential number must be obtained by counting entries (logical records) from the beginning, first entry = X00001, second = X00002, etc. (or first = C00001, second = C00002, etc. for the C-catalog, etc.). ------------------------------------------------------------------------------ Additional Information: If additional information about the XZ catalog is needed, contact Dr. David W. Dunham, IOTA, 7006 Megan Lane, Greenbelt, MD 20770-3012, Telephone: 301-953-5609; E-mail: dunham@nssdca.gsfc.nasa.gov A double precision function Fortran routine SECNDS is mentioned above; it converts a packed number in sexigessimal form, HHMMSS.SSS for R.A.'s and +/-DDMMSS.SS for declination, into a pure count of seconds from the origin. Another double precision function, SEX, does the inverse transformation from pure seconds to the packed sexigessimal form. These subroutines are listed below. Double Precision Function Secnds (A) C Convert D,M,S or H,M,S into seconds Double Precision A,B,C J = IDINT (1.D-4 * (A + DSIGN (1.D-4,A))) L = IDINT (A + DSIGN (1.D-4,A)) K = L - 10000 * J M = 40 * (90*J-K/100) + K B = M C = L Secnds = B + A - C Return End Double Precision Function Sex(X) C Convert number in seconds to sexigessimal form C X is in seconds. This function is the inverse of Secnds Implicit Real*8(A-H,O-Z) Data Ist/0/ If (Ist .gt. 0) Go to 10 Ist = 1 G = 1.D0 / 60.D0 H = G * G 10 A = DABS(X) B = A * H I = IDINT(B) C = I C C is integer degrees or hours A = A - 3600.D0 * C B = A * G I = IDINT(B) D = I C D is integer minutes A = A-60.D0 * D Sex = 10000.D0 * C + 100.D0 * D + A If (X .lt. 0.D0) Sex = -Sex Return End Changes to the catalog as received: This catalog and accompanying documentation were received from David Dunham in excellent shape. However, no decimal points were included (i.e., the decimal points were implicit.) As our current program to check catalogs does not handle implicit decimal points, the undersigned changed the formats to integer formats for checking. It was decided that these were unsuitable for general use, so the decimal points were inserted and the formats changed back to F formats. The zeros were omitted in the parallax, radial velocity, and SAO fields if no data were entered (i.e., the fields are blank). Wayne Warren subsequently moved the signs in the proper-motion and radial-velocity fields so that they always occur in the leftmost byte. He also added prefixes (BD, SD, CD) to the DM identifiers because both SD and CD stars occur in zone -22 degrees. I_201.xml The FK5 Extension on the FK4 System 1202 I/202 The FK5 Extension of the FK4 System The FK5 Extension on the FK4 System M G Lattanzi L G Taff Astron. J. 105 2353 1993 1993AJ....105.2353L Fundamental catalog The FK5 catalog was expanded from 1535 stars to include an additional 3117 stars which comprise the 'extension' to the new 'Basic' FK5, the revision of the FK4. For the basic FK5 a method of converting from the FK5 system to the FK4 system is provided in the catalog while for the Extension no algorithm was supplied. This catalog consists of two files. One file is the FK5 Extension placed at B1950.0 on the FK4 system. The second file is the FK5 Extension placed at the mean Epoch of place on the FK4 system.
FK5 Extension at B1950.0 on FK4 system FK5 Extension on the FK4 B1950.0 (Mean epoch of place) ID FK5 Extension ID number --- V V magnitude mag RAdh Right Ascension (B1950.0) in decimal hrs h DEdeg Declination (B1950.0) in decimal degrees deg Epoch_RA Mean Epoch of RA in decimal years yr Epoch_DEC Mean Epoch of DEC in decimal years yr pmRA Proper Motion in RA (B1950.0) sec/cy cs/yr pmDE Proper Motion in DEC (B1950.0) arcsec/cy carcsec/yr catalog.doc Description of the catalog N. Paul M. Kuin NASA/NSSDC/ADC 1996 Apr 08 Dr. Taff supplied the catalog documentation in printed form. This documentation was then keyed in at the ADC. I_202.xml Catalogue of Proper Motions, UBV-Photometry and Spectral Classification of the region of NGC 7092 (M39) 1203 I/203 Proper Motions, UBV-Phot. & Spectral Class Region 7092 Catalogue of Proper Motions, UBV-Photometry and Spectral Classification of the region of NGC 7092 (M39) I Platais Bull. Inf. CDS 44 9 1994 1994BICDS..44....9P Photometry, UBV Positional data Proper motions A catalogue of positions, proper motions and photographic UBV-magnitudes for 7931 stars in and around the open cluster NGC 7092 (M39) is presented. The Catalogue is complete down to B=16.0m and covers an area with diameter of ~110'. The spectral types are provided for 511 stars generally brighter than B=13.0m. For convenience, basic cross-identifications are also included. Refer to the file "intro.txt" for full details about the catalogue.
The Catalogue in the region of NGC 7092 SeqNo Sequential number of the star. --- NL Identification from Lavdovsky number=3 star number from Lavdovsky, 1961, Trudy Pulkovo Obs., Ser. 2, vol. 73, 5 (1961TrPul..73....5L); star numbers in his catalogue are increased by adding 1030. --- NAK Identification from Artiukhina+ number=4 Artiukhina and Kalinina, 1970, Trudy Sternberg Astron. Inst., vol. 40, 3 (1970TrSht..40....3A). This reference is also useful for finding the published Carte du Ciel numbers. --- NMS Identification from McNamara+ number=5 McNamara & Sanders, =1977A&AS...30...45M . A finding chart for all numbered stars is available. --- X Rectangular coordinate in millimeters number=1 Rectangular coordinates are derived from the ASCORECORD measurements of the deepest Pulkovo normal astrograph first-epoch plate B187 (scale=59.57"/mm; epoch=1909.65; equatorial coordinates at the optical center X=Y=0.0 mm: A=21 hours 32 minutes and 1.3 seconds, D=48 degrees 19 minutes and 34 seconds (J2000.0)). The X,Y-coordinate system is oriented reasonably close to the equatorial system at the equinox 1950.0. mm Y Rectangular coordinate in millimeters number=1 Rectangular coordinates are derived from the ASCORECORD measurements of the deepest Pulkovo normal astrograph first-epoch plate B187 (scale=59.57"/mm; epoch=1909.65; equatorial coordinates at the optical center X=Y=0.0 mm: A=21 hours 32 minutes and 1.3 seconds, D=48 degrees 19 minutes and 34 seconds (J2000.0)). The X,Y-coordinate system is oriented reasonably close to the equatorial system at the equinox 1950.0. mm pmX Relative proper motions in X number=2 The proper motions are determined relative to the mean of the field stars at about B=14.0m. 0.1mas/yr pmY Relative proper motions in Y number=2 The proper motions are determined relative to the mean of the field stars at about B=14.0m. 0.1mas/yr e_pm Mean standard error of proper motions number=6 Formal mean standard error of proper motions (equal errors in X- and Y-coordinate have been adopted). The mean error is calculated for an ensemble of stars in a limited magnitude interval and at a given position in the field. 0.1mas/yr Pr Calculated membership probabilities number=7 Calculated membership probabilities in percent for the cluster NGC 7092. All probable members of Anon (C2128+488) are marked with fake probabilities equal to "-99". % V Photographic UBV-photometry data. (see also n_UBV in byte 89) mag B-V Photographic UBV-photometry data. (see also n_UBV in byte 89) mag U-B Photographic UBV-photometry data. (see also n_UBV in byte 89) mag SpType Spectral types and luminosity classes. A finding chart for all classified stars is available in Platais (1988). --- Plate Designated plate numbers. An omitted pair number is replaced by zero --- n_XY "1" indicates that the X,Y-coordinates were transformed from another first-epoch plate into the system of plate B187. --- n_UBV "1" is set for all stars having corrupted UBV-photometry. --- RAh Right Ascension (hours), Equinox=J2000 and Epoch=J2000 h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Cross-identifications SeqNo The present Catalogue number. --- NEB Identification with Ebbighausen E.G., 1940, (1940ApJ....92..434E) --- NG Identification numbers from Glushkova E.V., 1991, Soviet Astron., vol 35, 466 (1991AZh....68..936G). Only a list of probable cluster members is available. --- NM Identification number from Maevers F.-W., 1940, Astron. Nachr., vol. 270, 201. (1940AN....270..201M) --- BD Bonner Durchmusterung <I/122> number. --- intro.txt Introduction to catalog by I. Platais Francois Ochsenbein CDS 1997 Feb 03 UNKNOWN UNKNOWN * 31-Jan-1994: first archived at CDS (Francois Ochsenbein) * 03-Feb-1997: standardized description I_203.xml The Bright Stars Supplement to the PPM and PPM South Catalogue, Revised Edition 1206 I/206 Bright Stars Supplement to PPM The Bright Stars Supplement to the PPM and PPM South Catalogue, Revised Edition U Bastian S Roeser Astronomisches Rechen-Institut, Heidelberg ??? ??? 1993 1993 I/146 : PPM-North Catalogue I/193 : PPM-South Catalogue I/208 : The 90000 stars Supplement to PPM Positional data Proper motions A number of bright stars is missing from the PPM Star Catalogue, both on the northern <I/146> and on the southern <I/193> hemisphere. The Bright Stars Supplement described here makes PPM complete down to V=7.5 mag. For this purpose it lists all missing stars brighter than V=7.6 mag that we could find in published star lists. Their total number is 275. Only 2 of them are brighter than V=3.5. This replaces the December 1992 edition (catalogue I/194) of the Bright Stars Supplement which inadvertently contained 46 duplicates of stars already contained in the main parts of PPM.
The Bright Star Supplement PPM PPM number 400196 is not in the HD. Its SAO number is 64296. --- DMcat Durchmusterung catalog abbreviation --- DMzone Durchmusterung zone --- DMno Durchmusterung number --- n_DMno Duplicity information for the DM number --- Vmag Visual magnitude mag RAh Right Ascension for the Equinox=J2000.0 and Epoch=J2000.0, on the system of FK5 h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination for the equinox and epoch J2000.0, on the system of FK5 deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec pmRA Proper motion in right ascension s/a pmDE Proper motion in declination arcsec/a HD HD Number --- n_HD HD component or duplicate indicator --- Flag1 'B' for Bright star --- Flag2 'D' for double star --- Flag5 'R' for Remark (only No 400148) explained in file descrip.txt --- descrip.txt Authors' description and remarks N. G. Roman ADC/SSDOO 1997 Nov 19 The original ReadMe was prepared by Joseph Florsch of the CDS and modified by Gail Schneider of the ADC. The version of the catalog that this described omitted the DM and SAO numbers, although there were spaces left for them. These were inserted by Wayne H. Warren, Jr, We thank Dr. Warren for forwarding his improved version to us. The original version also had several columns that were copied from the basic PPM catalog that did not contain useful information in this version. These have now been removed. I_206.xml A preliminary list of stars from Tycho observations 1207 I/207 Preliminary list from Tycho observations A preliminary list of stars from Tycho observations J L Halbwachs G Baessgen U Bastian D Egret E Hoeg F van Leeuwen C S Petersen P Schwekendiek A Wicenec Astron. Astrophys. 281, L25-L28 ??? ??? 1994 1994A&A...281L..25H I/196 : Hipparcos Input Catalogue, Version 2 (Turon+, 1993) I/197 : Tycho Input Catalogue, Revised version (Egret+ 1992) Positional data Magnitudes The selection of the stars of the Tycho program is mainly based on the Tycho input catalogue (TIC), prepared by Egret et al. (1992) from existing ground-based catalogues. The TIC is far to be the definitive list of the stars that will appear in the final Tycho catalogue however. The number of stars included within (3 million) is several times larger than the number eventually expected. The selection of the TIC stars that will remain in the final catalogue is planned in two steps : The former is the "Recognition" that is based on the first year of the scientific mission. The latter step of selection is the final reduction of the Tycho data, which will require a few more years. The recognition was completed in 1992, and, among the 3,154,204 stars of the TIC, about two third were not found in the observations. This catalogue presents the 1,049,971 stars that are still in the programme. The selection is nor definitive, nor complete; but it should contain only a small percentage of stars that will still be discarded. On another side, some stars missing in the TIC have been added to the Tycho program, but the expected number of additional stars to appear in the final catalogue should be about 5 % or less. The list was announced in Halbwachs et al (1994). It is completed with data (coordinates and magnitudes) from the main file of the Tycho Input Catalogue. The cross-identifications with the Hipparcos Input Catalogue or with the INCA database included in catalogue I/197/ are not repeated here.
The catalogue TICID1 GSC region number --- TICID2 GSC running number in region --- RA10mas Right ascension J2000.0, Epoch=1990, in 0.01arcsec 10mas SPD10mas South Polar Distance (=Dec+90) Epoch 1990, in 0.01arcsec 10mas e_pos Error on position in 0.01arcsec 10mas e_B Error on B mag. in 0.01 mag. (0=unknown) .01mag B B magnitude in 0.01 mag. (0=unknown) .01mag e_V Error on V mag. in 0.01 mag. (0=unknown) .01mag V V magnitude in 0.01 mag. (0=unknown) .01mag Flag1 FK5 star --- Flag2 IRS star --- Flag3 Photometric standard for Tycho --- Flag4 Monitor star : random set --- Flag5 Monitor star : selected from TIC flags --- Flag6 Monitor star : NGC, ADS system --- Flag7 Photometric star --- Flag8 Monitor star (logical OR of #1 to #6) --- Flag9 GSC/INCA discrepancy --- Flag10 Star selected in the Recognition process --- Flag11 GSC/INCA magnitude discrepancy --- Flag12 INCA (or CDA) entry NOT in GSC 1.0 --- Flag13 Source of position (0: GSC; 1: INCA) --- Flag14 -id.- for B magnitude --- Flag15 -id.- for V magnitude --- Flag16 Non-stellar GSC image ("unknown" class) --- Flag17 Component of TIC pair (sep < 20") --- Flag18 Close pair with one single entry (sep < 3") --- Flag19 Component of INCA pair (sep < 10") --- Flag20 INCA/CDA star (cross-id. in Annex file) --- Flag21 Known proper-motion --- Flag22 Known high proper-motion (>0.15"/yr) --- Flag23 Known parallax --- Flag24 Known variable --- Flag25 Known multiple system --- Flag26 Hipparcos Input Catalogue star (Annex file) --- Flag27 CDA star (complementary astrometric data) --- Jean-Louis Halbwachs CDS 1995 Nov 04 UNKNOWN UNKNOWN * 10-Jan-1994: Original file written by Jean-Louis Halbwachs [CDS] * 04-Nov-1995: This file revisited at CDS (mainly cosmetics) I_207.xml The 90000 Stars Supplement to the PPM Star Catalogue 1208 I/208 90000 Stars Supplement to the PPM Star Catalogue The 90000 Stars Supplement to the PPM Star Catalogue S Roeser U Bastian A V Kuzmin Astron. Astrophys. Suppl. Ser. 105 301 1994 1994A&AS..105..301R Positional data Proper motions Since its appearance in 1966, the SAO Catalogue (SAO, 1966) has been the primary source for stellar positions and proper motions. Typical values for the rms errors are 1 arcsec in the positions at epoch 1990, and 1.5 arcsec/century in the proper motions. The corresponding figures for the AGK3 (Heckmann et al., 1975) on the northern hemisphere are 0.45 arcsec and 0.9 arcsec/century. Common to both catalogues is the fact that proper motions area derived from two observational epochs only. Both catalogues are nominally on the B1950/FK4 coordinate system. The PPM Star Catalogue (Roeser and Bastian, 1991, Bastian et al., 1993; for a short description see Roeser and Bastian, 1993) effectively replaced these catalogues by providing more precise astrometric data for more stars on the J2000/FK5 coordinate system. Compared to the SAO Catalogue the improvement in precision is about a factor of 3 on the northern and a factor of 6 to 10 on the southern hemisphere. In addition, the number of stars is increased by about 50 percent. Typical values for the rms errors on the northern hemisphere are 0.27 arcsec in the positions at epoch 1990, and 0.42 arcsec/century in the proper motions. On the southern hemisphere PPM is much better, the corresponding figures being 0.11 arcsec and 0.30 arcsec/century. The improvement over the SAO Catalogue was made possible by the advent of new big catalogues of position measurements and by the inclusion of the century-old Astrographic Catalogue (AC) into the derivation of proper motions (for a description of AC see Eichhorn, 1974). But even PPM does not fully exploit the treasure of photographic position measurements available in the astronomical literature of the last 100 years. The Astrographic Catalogue contains roughly four million stars that are not included in PPM. For most of them no precise modern-epoch position measurements exist. Thus it is not yet possible to derive proper motions with PPM quality for all AC stars. But among the 4 million there is a subset of some 100,000 CPC-2 stars that are not included in PPM. These stars constitute the 90,000 Stars Supplement to PPM.
The catalogue PPM Designation of the star Designation of the star in PPM South starting with No. 181732, see chapter 3 of description file. --- DM BD (zones -02 to -22), else CD Designation of the star in the Bonner Durchmusterung (for zones from -02 to -22 degrees) or in the Cordoba Durchmusterung (zones -23 to -89 degrees). --- mag Magnitude See chapter 3 of description file. mag Sp Spectral type --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec pmRA Proper motion in RA, J2000 Proper motion in right ascension for epoch and equinox J2000.0, on the system of FK5 given in seconds of time per Julian year. s/yr pmDE Proper motion in DE, J2000 arcsec/yr N Number of individual published positions used Number of individual published positions used for the derivation of the position and proper motion given. --- e_RA Mean error of RA Mean error of right ascension at the mean epoch right ascension, multiplied by the cosine of declination, given in units of #0.01 seconds of arc. 10mas e_DE Mean error of DE Mean error of right ascension at the mean epoch of declination, given in units of #0.01 seconds of arc. 10mas e_pmRA Mean error of pmRA Mean error of the proper motion in right ascension, multiplied by the cosine of declination, given in units of 0.001 second of arc per Julian year. mas/yr e_pmDE Mean error of pmDE Mean error of the proper motion in declination, given in units of 0.001 seconds of arc per Julian year. mas/yr EpRA Weighted mean epoch, RA and pmRA Weighted mean epoch of the measured positions used for the derivation of RA and pmRA, given in years since 1900.0. yr EpDE Weighted mean epoch, DE and pmDE Weighted mean epoch of the measured positions used for the derivation of DE and pmDE, given in years since 1900.0. yr SAO SAO Designation --- HD Henry Draper Designation --- CPD Cape Photographic Durchmustrung Designation --- Flag1 'P' - problem, 'C' - comment P - problem case, preferably not to be used as astrometric reference star. C - a critical comment is given in the List of Critical Comments. Not to be used as astrometric reference star. --- Flag2 'D' - double star D - double star, preferably not to be used as astrometric reference star. --- Flag3 - not used Not used, void for consistency with PPM (north). --- Flag4 'F' - member of FK5 F - member of FK5, mostly bright stars, original FK5 data are given. --- Flag5 'R' - remark, 'V' - V mag (CPC-2) R - a remark is given in the List of Remarks on Individual Stars. V - the magnitude is a photographic V magnitude copied from CPC-2. --- descrip.doc Authors' description Michel Creze CDS Gail L. Schneider NSSDC/ADC 1994 Nov 11 I_208.xml Catalogue of the Components of Double, Multiple stars (CCDM) first edition 1211 I/211 CCDM Catalogue of the Components of Double, Multiple stars (CCDM) first edition J Dommanget O Nys Comm. Obs. R. Belgique, Ser. A, N. 115 ??? ??? 1994 1994CoORB.115....1D I/196 : Hipparcos Input Catalogue Stars, double and multiple The introduction to this catalogue has been the subject of a publication in the "Communications de l'Observatoire Royal de Belgique" (Serie A, number 115). Detailed are: its origins, its aims, its realization, the search of identifiers, the compilation of astrometric data and the related problems as well as the fundamental ties between the CCDM and the HIPPARCOS INPUT CATALOGUE (HIC). It also contains a complete bibliography of the referred papers. The contents of the general catalogue (63,463 systems) is also described as well as the conditions of its availability to the astronomical community and the projects underway for the next edition. For all these items, the user is invited to refer to this publication because hereafter only the format and the contents of the catalogue follow. To identify the systems and their components, we adopted the clever numbering process of the authors of the INDEX consisting in combining the right ascension and declination, respectively limited to 0.1 minute of time and to 1 minute of arc. In order to distinguish the CCDM numbers from the INDEX numbers - in addition to their different equinox: 2000 for the CCDM and 1900 for the INDEX - we adopted the signs + and - instead of the letters N and S for separating the coordinates. Consequently, in the INDEX and in the CCDM, one entry is devoted to a same system but the contrary to the INDEX, where a sub-entry is assigned to each group of two components, whatever the multiplicity of the system may be, the CCDM allows one sub-entry and thus one record per component. The present edition contains only the 34,031 systems (table below, part I) for which an accurate position has been found for at least one component. The catalogue extends thus much over the sample of the somewhat 14,000 systems finally retained for the HIPPARCOS INPUT CATALOGUE and assembled in its Annex 1.
The Catalogue CCDM (Catalogue of the Components of the Double and Multiple stars) number number=1 The CCDM number is made with RA(2000) limited to 0.1 minute of time (HHMMm) and Dec(2000) limited to 1 minute of a degree (+DDMM). Full details about the construction of the CCDM number are given in the publication. --- rComp Reference component (blank if A) number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- Comp Concerned component In one record there appear '?' signs for (CCDM#=) 07366-1428 number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- Note1 *=orbit in Dommanget's personal cat. number=2 The personal catalogue of J.Dommanget (1982; partially updated to 1994) --- Note2 @ = astrometric binary number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- Disc Name of the pair (Discoverer and Number) number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- dRAs Remainder of RA in second of time; number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 s dDEs Remainder of DE in arcsecond; number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 arcsec r_dRAs Source code for positions number=3 See the document file, part III --- Year Year of measured relative position number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 yr theta Position angle (degrees) number=4 The following letters are sometimes used to indicate an approximate location of the secondary component: 'N' (to the North) 'NF'(to the North and following) (first quadrant) 'F' (following) 'SF'(to the South and following) (second quadrant) 'S' (to the South) 'SP'(to the South and preceding) (third quadrant) 'P' (preceding) 'NP'(to the North and preceding) (fourth quadrant) deg rho angular separation of Comp along theta number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 arcsec Obs for A component: number of components; other component: number of measurements number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- Vmag magnitude number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 mag Sp spectrum number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- pmNote Origin of the proper motion *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- pmRA annual proper motion in 0"001 number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 mas pmDE annual proper motion in 0"001 number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 mas DM First identification = DM (Harvard system) number=5 .0 = BD .6 = AGK2/3 .2 = CD .8 = SAO .4 = CPD The suffixes "a" and "b" following some DM designations appear in place of the dot. --- Name2 Second identification number=5 .0 = BD .6 = AGK2/3 .2 = CD .8 = SAO .4 = CPD The suffixes "a" and "b" following some DM designations appear in place of the dot. --- HD HD designation number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- m_HD second HD (Example: 131843/4) number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- ADS/BDS ADS number (A) or BDS number (B) number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- m_ADS/BDS suffix (a) to an inserted ADS number number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- n_IDS The * means that the Index number is built for new component or system; number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- IDS Uncorrected Index designation (1976.5) (equinox 1900) and identification letter; number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- HIC Hipparcos Input Catalogue (Turon et al.) number number= *: not the pm from the Index; @: pm from the HIC; $: pm = pm(B/A); number= In one record there appear '?' signs for (CCDM#=) 07366-1428 --- ccdm.doc Documentation J. Dommanget Obs. Royal Bruxelles 1996 Nov 14 UNKNOWN UNKNOWN Editing of the original ReadMe (1994) was done at the NASA/ADC. I_211.xml Catalogue of Proper Motions in the region of NGC 3680. 1212 I/212 Proper motions in NGC 3680 Catalogue of Proper Motions in the region of NGC 3680. V Kozhurina-Platais T M Girard I Platais W F van Altena P A Ianna R D Cannon Bull. Inf. CDS 46 9 1995 1995BICDS..46....9K Clusters, open Positional data Proper motions Magnitudes, photographic A catalogue of positions, proper motions and photographic BV magnitudes for 2711 stars in and around the open cluster NGC 3680 is presented. The Catalogue is complete down to B=17.5 mag in a rectangular, one square degree area centered on the cluster. The limiting magnitude of the Catalogue is B=18.4 mag. The mean standard error of the proper motions for well-measured stars is +/-0.35 mas/yr. The photographic B and V magnitudes are accurate to about +/-0.1 mag. The mean error of the relative positions for all 2711 is +/-0.025 arcsec at the mean epoch of the plate material, 1977.8. For each star, three different cluster membership estimators are presented. For convenience, cross-identifications to other studies are provided.
The open cluster NGC 3680 (C1123-429; l=286.8 deg, b=16.9 deg) fits the same age group as the well-studied cluster M67, although it is not a twin of that cluster. For instance, NGC 3680 contains a much smaller number of cluster members. Most likely it belongs to the group of so-called poorly-populated open clusters which has been studied by Platais (1994). Unfortunately, the lack of an astrometric study before now, impeded reaching definite conclusions as to the cluster's basic parameters and the luminosity function. Recently Kozhurina-Platais et. al (1995) have completed a comprehensive proper motion study of NGC 3680. Here we present an extended version of the proper motion catalogue for all 2711 stars measured in that study. The Catalogue should prove valuable for further studies of the cluster properties and also can be useful for galactic structure studies toward the galactic anti-rotation direction as demonstrated by Mendez et al. (1993). Data description: A detailed description of the astrometric and photometric data is available in Kozhurina-Platais et al. (1995). Only a brief summary of the reductions and attained accuracies is provided here. The astrometric reductions were based on twelve plates taken with the Yale-Columbia 26-in refractor (plate scale 18.85 "/mm). The earliest plate was taken in 1947, the latest - 1992. The largest plates cover 67' (E-W) by 52' (N-S) area. All of the plates were digitized with the Yale PDS microdensitometer equipped with laser encoders. Image centroids were obtained by fitting a two-dimensional bivariate Gaussian to the image density profiles. Proper motions were calculated using the basic principles of an iterative central-plate overlap technique supplemented with a very careful account of the magnitude equation and the magnitude/color corrections. Relative proper motions were calculated for 2711 stars, measured on at least three plates which spanned a minimum of ten years epoch difference. The standard error of the proper motion for bright (V<14.0 mag) stars, measured on all twelve plates, is +/-0.35 mas/yr. The Catalogue of proper motions is complete down to B=17.5 mag, while the limiting magnitude is B=18.4 mag. The five best 26-in telescope plates were used to obtain the B magnitudes. V magnitudes were derived primarily from two visual Yale Southern Observatory 51-cm astrograph plates. The instrumental magnitudes were transformed into the standard BV magnitudes using photographic BV-photometry by Anthony-Twarog et al. (1991). The formal photometric error for the whole Catalogue is about +/-0.1 mag in both B and V magnitude. Our BV photometry should be used with caution in a detailed analysis of the cluster's color-magnitude diagram since its primary purpose was for application of magnitude and color corrections made in the astrometric reductions. We are aware of several stars with totally erroneous V-photometry (for instance, Nos. 376, 2696) caused by the difficulty in separating blended images on the 51-cm astrograph visual plates. In addition to the proper motion, we also present each star's mean position. The mean error of the relative positions for all 2711 stars is +/-0.45 micron or, in corresponding angular units, +/-0.025 arcsec, and for the 524 stars brighter than V=14.5 mag, the internal error is +/-0.18 micron (+/-0.010 arcsec) at the mean epoch of the plate material, 1977.8. Note that we had no control over possible magnitude equation in the positions. The mean positions were updated to epoch=2000.0 and then transformed into the HST Guide Star Catalog system of celestial coordinates using 219 reference stars. The unit weight mean error of this transformation is +/-0.18 arcsec, which is dominated by the errors in the reference frame. Proper motion errors: In the Catalogue the single-coordinate proper-motion formal error is estimated from the scatter about the best-fit line for each star separately. Due to the small number of plates involved in the solution, this formal error may not always be a statistically reliable estimator of the true error. Here we would like to caution that the proper motion uncertainties given in Kozhurina-Platais et al. (1995) for the probable cluster members are calculated by median smoothing the proper-motion error distribution as a function of B magnitude. This procedure, however, was not applied to the stars with proper-motion errors exceeding three times the median-smoothed error estimate. The proper-motion membership probability calculation benefited significantly from the use of these median-smoothed proper-motion error estimates. Statistical properties of the formal errors, though, should be studied only from the error values provided in this Catalogue. Membership Probabilities: The probability of a given star being a cluster member is defined as the ratio of the frequency of cluster stars to all stars at the point within the proper motion distribution corresponding to that star's proper motion. To derive the probabilities, the standard technique (Sanders, 1971) of modeling the proper-motion distributions has been widely used. Following this tradition, we applied the modified Sanders method to the proper-motion data and derived the probabilities P_\mu. Our best fit to the proper-motion distributions yields only 74 cluster members. With such a small fraction of cluster members, the associated membership probabilities may be sensitive to the shape of cluster's luminosity function and the spatial distribution. The latter can be rigorously taken into account by including an empirical spatial surface density distribution into the membership probability. The joint spatial/proper motion membership probabilities P_\mu,r provide more realistic probability estimates but can be distorted by a varying cluster-to-field luminosity function ratio over the entire magnitude range. Therefore, we also provide a so-called local-sample membership estimator, P_s, which should not be biased by possible differences in the shape of the luminosity functions. Note that these probabilities are calculated only for stars measured on seven or more plates. For practical cluster member selection purposes, we recommend use of the P_\mu,r probabilities with the caution not to use them to derive information regarding the cluster's spatial structure. A full discussion regarding the various membership probability estimates can be found in Kozhurina-Platais et al. (1995).
The catalogue of stars in NGC 3680 No Sequential number of the star. --- Vmag Photographic BV-photometry. mag B-V Photographic colour index mag RAh Right Ascension (hours) Equinox=J2000, Epoch=J2000 h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec nPlates The number of plates used in the proper motion calculation. --- pmX Relative proper motions in X-coordinate. mas/yr pmY Relative proper motions in Y-coordinate. mas/yr e_pmX Formal error of pmX. mas/yr e_pmY Formal error of pmY. mas/yr Pr(pm) Standard membership probability for the cluster NGC 3680. number=2 see above section on Membership Probabilities % Pr(pm,r) Joint spatial/proper motion membership probability. number=2 see above section on Membership Probabilities % Pr(S) =-1 Local-sample membership probability; negative probabilities indicate a not computed probability. number=2 see above section on Membership Probabilities % X Standard-plate coordinate number=1 Mean standard-plate coordinates derived from the iterative central-plate overlap solution (epoch=1977.8, scale=18.85 "/mm). The mean standard plate originated from the plate #Y36 with X=Y=0.0 placed close to the optical center. mm Y Standard-plate coordinate number=1 Mean standard-plate coordinates derived from the iterative central-plate overlap solution (epoch=1977.8, scale=18.85 "/mm). The mean standard plate originated from the plate #Y36 with X=Y=0.0 placed close to the optical center. mm e_X Mean error on X (microns) um e_Y Mean error on Y (microns) um Cross-identifications with previous work No The present Catalogue number. --- Ant-Twa Identification with Anthony-Twarog et al. (1991). --- Eggen Identification with Eggen (1969). --- Francois Ochsenbein CDS 1995 Feb 08 E-mail (for the first author): vera@astro.yale.edu I_212.xml Lick Northern Proper Motion Program: NPM1 Catalog Cross-Identifications and Appendices 1214 I/214 NPM1 Cross Index Lick Northern Proper Motion Program: NPM1 Catalog Cross-Identifications and Appendices A R Klemola R B Hanson B F Jones Bull. American Astron. Soc., 184, #27.07 ??? ??? 1994 1994AAS...184.2707H Cross identifications Proper motions The NPM1 Catalog provides absolute proper motions, positions, and photographic photometry, measured in the Lick Northern Proper Motion (NPM) program, for some 149,000 stars in the magnitude range 8 < B < 18 mag. covering the sky outside the Milky Way north of 23 deg declination. The NPM1 Cross-Identifications file provides some 42,000 cross-identifications between the NPM1 Catalog numbers and star names, stellar type classifications, and publication references. These additional data, extracted from the Lick Input Catalog of Special Stars, facilitate many practical uses of the NPM1 Catalog. Six Appendices to the NPM1 Catalog provide references, footnotes, and other useful information.
the NPM1 Catalog Cross Identifications file zonesign NPM1 star "name" (bytes 1-8) made of: Sign of declination for this zone --- zone Declination zone deg dot dot separator --- num Running number in this declination zone --- starname Name of star (from literature source) --- class Code for class of object (npm1code.dat) --- r_NPM1 Publication reference number (npm1refs.dat) --- n_NPM1 Code for notes: 0= no comment 1= identification uncertain 2= reject (npm1rej.dat) 3= footnote (npm1foot.dat) --- mag 0.00 Magnitude quoted from publication reference; zero if none mag ci 0.00 B-V color quoted from publication reference; zero if none mag magType Magnitude type: 0= none, 1= V, 2= B, 3= mpv, 4= mpg, 5= other --- n_ci Color-index type: 0= none, 1= B-V. --- ref Publication reference (npm1refs.dat) --- Appendix 1 object class codes translation class Code for class of object (npm1cross.dat) --- eq equal sign --- trans Translation of class code into star type --- Appendix 3 abbreviated references identification r_NPM1 Publication reference number --- ref Publication reference (npm1cross.dat) --- numstars Number of stars from this reference in NPM1 --- code1 Codes for classes found in this reference --- code2 Codes for classes found in this reference --- code3 Codes for classes found in this reference --- code4 Codes for classes found in this reference --- code5 Codes for classes found in this reference --- code6 Codes for classes found in this reference --- code7 Codes for classes found in this reference --- code8 Codes for classes found in this reference --- Appendix 4 full references in ascii format r_NPM1 publication reference code blank = continuation --- ref reference text --- Appendix 5 footnotes to the NPM1 catalog zonesign NPM1 star "name" (bytes 1-8) made of: Sign of declination for this zone --- zone Declination zone deg dot dot separator --- num Running number in this declination zone --- note either the footnote text (npm1foot.dat) or the reason for rejection (npm1rej.dat) --- Appendix 6 18 stars to be rejected from the NPM1 zonesign NPM1 star "name" (bytes 1-8) made of: Sign of declination for this zone --- zone Declination zone deg dot dot separator --- num Running number in this declination zone --- note either the footnote text (npm1foot.dat) or the reason for rejection (npm1rej.dat) --- npm1cros.tex Full documentation [NSSDC/WDC-A-R&S 94-14] npm1code.txt Appendix 2 object class codes grouped npm1refs.tex Appendix 4 full references in LaTeX format npm1refs.txt Appendix 4 full references in ascii format Bob Hanson UCO/Lick Obs. and Paul Kuin ADC 1995 Apr 06 UNKNOWN UNKNOWN 28-Nov-1994 I_214.xml Tables of membership for 43 open clusters (1994 Version) 1215 I/215 Tables of membership for 43 open clusters Tables of membership for 43 open clusters (1994 Version) J -L Zhao K P Tian Bull. Inf. CDS 47 5 1995 1995BICDS..47....5Z Clusters, open Proper motions Relative proper motion data have been widely used to determine membership of open clusters. In view of the fact that most of data of proper motions had been obtained before Sanders' method was set up and information on membership of open clusters had been mostly published without a statistically rigorous method available, it is necessary to restudy membership of clusters from data by means of the rigorous method. 59 pieces of relative proper motion data for 43 open clusters having been collected, we, by use of the improved Sanders' method, calculate membership probabilities of all the stars for each field, based upon which individual member stars are found. Recently we have obtained proper motions and membership of open clusters of M67, NGC2286 and Orion, which are also included in this new version. All the results concerned are given in the form of catalogue.
List of Clusters Seq Order number --- Cluster Name of open cluster --- File Name of file --- Nstars Total number of stars (1st line) --- Nmembers Number of cluster member number=1 the next line lists the uncertainty on the parameter --- pmX(fld) Proper motion of field center in X number=1 the next line lists the uncertainty on the parameter 10mas/yr pmY(fld) Proper motion of field center in Y number=1 the next line lists the uncertainty on the parameter 10mas/yr pmX(cl) Proper motion of cluster center in X number=1 the next line lists the uncertainty on the parameter 10mas/yr pmY(cl) Proper motion of cluster center in Y number=1 the next line lists the uncertainty on the parameter 10mas/yr sdX(fld) Standard deviation in X of field stars number=1 the next line lists the uncertainty on the parameter 10mas/yr sdY(fld) Standard deviation in Y of field stars number=1 the next line lists the uncertainty on the parameter 10mas/yr sd(cl) Standard deviation of cluster stars number=1 the next line lists the uncertainty on the parameter 10mas/yr PA Rotation angle to the major axis of the field distribution deg Ref Reference --- Berkeley 58 IC 1805 IC 4665 IC 4756 NGC 129 NGC 129 NGC 129 NGC 188 NGC 457 NGC 581 NGC 581 NGC 663 NGC 752 NGC 1664 NGC 1817 NGC 1912 NGC 2099 NGC 2099 NGC 2099 NGC 2168 NGC 2168 NGC 2264 NGC 2281 NGC 2286 NGC 2420 NGC 2548 NGC 2682 NGC 2682 NGC 2682 NGC 2682 NGC 6611 NGC 6633 NGC 6705 NGC 6705 NGC 6705 NGC 6811 NGC 6819 NGC 6823 NGC 6882 NGC 6885 NGC 6913 NGC 6939 NGC 7062 NGC 7092 NGC 7092 NGC 7092 NGC 7209 NGC 7654 NGC 7788 NGC 7788 NGC 7790 Orion Nebula h Per chi Per Trumpler 1 Trumpler 1 Number The star number --- x_mag Filter Indicator number=1 x_mag takes the following values: 'B' if "mag" column contains the B magnitude 'V' if "mag" column contains the V magnitude 'P' if "mag" column contains a photographic magnitude 'D' if "mag" column contains a stellar diameter expressed in mm --- n_mag Note v=very faint f=faint --- mag Stellar magnitude or diameter number=1 x_mag takes the following values: 'B' if "mag" column contains the B magnitude 'V' if "mag" column contains the V magnitude 'P' if "mag" column contains a photographic magnitude 'D' if "mag" column contains a stellar diameter expressed in mm --- var v=variable --- X The measured coordinates in X mm Y The measured coordinates in Y mm pmX Proper motion in X 10mas/yr pmY Proper motion in Y 10mas/yr Pr Membership probabilities --- oriNumber The number in the original data --- e_pmX Mean error on pmX 10mas/yr e_pmY Mean error on pmY 10mas/yr NGC 6530 NGC 654 Orion Nebula Number The star number --- x_mag Filter Indicator number=1 x_mag takes the following values: 'B' if "mag" column contains the B magnitude 'V' if "mag" column contains the V magnitude 'P' if "mag" column contains a photographic magnitude 'D' if "mag" column contains a stellar diameter expressed in mm --- n_mag Note v=very faint f=faint --- mag Stellar magnitude or diameter number=1 x_mag takes the following values: 'B' if "mag" column contains the B magnitude 'V' if "mag" column contains the V magnitude 'P' if "mag" column contains a photographic magnitude 'D' if "mag" column contains a stellar diameter expressed in mm --- var v=variable --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec pmX Proper motion in X 10mas/yr pmY Proper motion in Y 10mas/yr Pr Membership probabilities --- oriNumber The number in the original data --- e_pmX Mean error on pmX 10mas/yr e_pmY Mean error on pmY 10mas/yr Francois Ochsenbein, Joseph Florsch CDS 1995 Mar 28 I_215.xml Positions, proper motions, and magnitudes in the area of the open Cluster Tr 10. 1216A I/216A Open cluster TR 10 Positions, proper motions, and magnitudes in the area of the open Cluster Tr 10. J Stock Rev. Mex. Astron. Astrofiz. 9 127 1984 1984RMxAA...9..127S Clusters, open Proper motions Positions for 979 stars in the area of Tr 10 are derived from fifteen plates taken recently with the ICDA refractor. For the determination of proper motions nine plates of the Cape Astrographic Catalogue are used as first epoch. The results make it appear doubtful that the object is a single cluster.
The catalogue Seq Running number --- RAh Right ascension Equinox=1950.0, Epoch=1982.4 h RAm Right ascension Equinox=1950.0, Epoch=1982.4 min RAs Right ascension Equinox=1950.0, Epoch=1982.4 s DE- Declination sign --- DEd Declination Equinox=1950.0, Epoch=1982.4 deg DEm Declination Equinox=1950.0, Epoch=1982.4 arcmin DEs Declination Equinox=1950.0, Epoch=1982.4 arcsec Vmag Visual magnitude derived from CIDA plates mag o_Vmag Number of images measured from CIDA plates --- PMag Photographic magnitude derived from Cape plates mag o_PMag Number of images measured on Cape plates --- pmRA Proper motion in right ascension 0.1mas/yr pmDE Proper motion in declination 0.1mas/yr Marie-Jose Wagner, Patricia Bauer CDS 1995 May 05 UNKNOWN UNKNOWN Keypunched at CDS * 08-Dec-1994: First archived * 05-May-1995: 7 errors detected by J.C. Mermilliod <mermio@scsun.unige.ch> in declinations of # 236, 275, 571, 613, 618, 633, 767 I_216A.xml The Magellanic Catalogue of Stars - MACS 1221 I/221 The Magellanic Catalogue of Stars - MACS The Magellanic Catalogue of Stars - MACS H -J Tucholke K S De Boer W C Seitter Astron. Astrophys. Suppl. Ser. 119 91-98 1996 1996A&AS..119...91T The Magellanic Catalogue of Stars - MACS H -J Tucholke K S De Boer W C Seitter The Messenger 81 20 1995 1995Msngr..81...20D Magellanic Clouds Positional data The Magellanic Catalogue of Stars (MACS) is based on scans of ESO Schmidt plates and contains about 244,000 stars covering large areas around the LMC and the SMC. The limiting magnitude is B<16.5m and the positional accuracy is better than 0.5" for 99% of the stars. The stars of this catalogue were screened interactively to ascertain that they are undisturbed by close neighbours.
The Large Magellanic Cloud The Small Magellanic Cloud MACS Designation --- RAh Right Ascension J2000 , Epoch 1989.0 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 , Epoch 1989.0 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Npos Number of positions used --- Mag Instrumental Magnitude (to be used only in a relative sense) mag PosFlag Position Flag (0: ok, 1: internal error larger than 0.5") --- MagFlag Megnitude Flag (0: ok, 1: bad photometry or possible variable) --- BochumFlag Bochum Flag 1 if in Bochum catalog of astrophysical information on bright LMC stars) (yet empty) --- Hans-Joachim Tucholke Univ. Bonn 1995 Nov 20 Author's address: Hans-Joachim Tucholke <tucholke@astro.uni-bonn.de> I_221.xml The Washington Visual Double Star Catalog, 1996.0 1237 I/237 The Washington Visual Double Star Catalog, 1996.0 The Washington Visual Double Star Catalog, 1996.0 C E Worley G G Douglass US Naval Observatory ??? ??? 1996 1996 The Washington Visual Double Star Catalog, 1996.0 C E Worley G G Douglass Astron. Astrophys. Suppl. Ser. 125 523 1997 1997A&AS..125..523W I/211 : CCDM (Components of Double and Multiple stars) (Dommanget+ 1994) Stars, double and multiple Positional data The Washington Visual Double Star Catalog, 1996.0 (WDS) is the successor to the catalog of the same name dated 1984 <I/107>. The WDS is intended to contain all known visual double stars for which at least one differential measure has been published through the end of 1995. It includes a discoverer code, the date of the first and last observations, the number of observations, the position angle and separation for the first and last observation, the magnitudes and spectral types of the components (when available) the proper motion of the system, Durchmusterung numbers of the components and notes for further information.
The reader is reminded that the WDS is not inclusive of all pairs which have been more casually noted, although it does, in fact, include some of them. The data base upon which the present WDS rests consists of the approximately 180000 measures transferred from the Lick Observatory in 1965, which, with few exceptions, covered the interval 1927-1963, augmented by all subsequent measures (about 118000), and some 154000 pre-1927 means. These latter are the result of a continuing project to build a truly comprehensive and complete data base. Thus, approximately 452000 individual means, representing over a million individual observations, form the basic material from which the WDS is constructed. We have not included a small amount of data because of unresolved questions concerning it. The WDS contains 78100 double stars, counting, as did the IDS, multiple components in the same system as separate pairs. Comparison of the present catalog with its IDS predecessor will reveal that a considerable number (about 1000) of previously catalogued objects have been removed from the WDS in the process of editing the data. The most common reason for removal is that the object is not certainly double. We wish to emphasize that the WDS is not intended to be an "astrometric" catalog in the sense usually employed, but rather is to be considered a finding list for observers, as well as serving as a notification of which objects are known doubles or multiples, along with some basic astrometric and astrophysical parameters. In addition, the WDS offers information on the amount of motion and frequency with which a given object has been observed, which is sufficient, in fact, to provide a basis for the construction of observational programs. Finally, the data can be used (with proper precautions) to analyze certain statistical properties of visual double stars. Of course, as has been true for many years, the individual measures of specific objects are available and will be supplied to requesters provided that the amount of data desired is reasonable.
WDS Catalog RAh Right Ascension 2000 (hours) The positions given represent our best estimates of these values. Where possible, these are based on the ACRS and PPM data, with proper motion incorporated. (Code "p" in cols. 79-80). h RAdm Right Ascension 2000 (minutes) 0.1min DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DiscName Discoverer Code & Number The discoverer, identified by a one-to-three letter code, and the discoverer's number, if assigned. The reference list ("wdsref.dat") should be consulted first to identify individuals. However, some discoverer designations do not appear in this list, for various reasons, and a supplementary list is provided (wdsrefa.dat"). --- Comp Component Identification Components, when the object has more than two. The Lick IDS scheme has been discontinued, and components are now referred to by the traditionally employed lower-case letters. The rather awkward upper-case designations, e.g. ABXC, have been changed to the form AB-C, etc. We have noted some confusion on the part of observers and students alike, as to how to designate components in multiple systems. Traditionally, these have been designated in order of separation, thus AB, AC,...., or in the cases where close pairs are observed blended, AB-C, AB-D,.... In some instances, differing resolution limits produce situations where observations are intermixed, thus AC, AB-C, and so forth. (In all too many cases, carelessness on the part of the observer does not permit us to determine with certainty how the observation is to be interpreted). There are also many instances where later observations have revealed a closer companion; these are designated Aa, Bb, etc. In a few cases wider, later discoveries have also been so denoted. --- Date1 Date of first satisfactory observation (+1000) a Date2 Date of last satisfactory observation (+1000) a NumObs Number of measures of the object The number of measures of the object. When there are more than 99, the number 99 is used. For smaller numbers of observations, the value in these columns is intended to accurately reflect the actual number. --- pa1 Position Angle for Date1 Position angles in degrees for the dates listed in columns 24-29. For some pairs, the discoverers have given only crude estimates, such as NF or SP; in such cases these are listed. Position angles are unprecessed in this catalog (i.e. they are for the mean date of observation). deg pa2 Position Angle for Date2 deg Sep1 Angular Separation for Date1 The distances in seconds of arc, and tenths, for the dates listed in columns 24-29. Some separations are treated by the codes found in columns 79-80, or in the Notes. In cases where there has been no appreciable motion observed over the duration of observation, only one position angle and separation is listed. arcsec Sep2 Angular Separation for Date2 arcsec MagA Magnitude of component 1 mag MagB Magnitude of component 2 mag Sp Spectral Types of Primary/Secondary Spectral type of A, or of two components, if space permits. (See "wdscat.doc" for discussion). --- pmRA Proper Motion in Right Ascension The components of the proper motion in seconds of arc per 1000 years, in right ascension reduced to great circle, and in declination. Specifically, this catalog lists 15mu(alpha)*cos(delta), where mu(alpha) is in seconds of time, and mu(delta) is in seconds of arc. Both quantities are reduced to a time unit of 1000 years. The exceptions are those objects coded P, Q, and R, for which an explanation is given under the description for Columns 79 and 80. + and - indicate eastward and westward motions in Right Ascension, and + and - those north and south in Declination. mas/a pmDE Proper Motion in Declination mas/a DM Durchmusterung Zone & Number Durchmusterung number of the object in the system used by the Henry Draper Catalogue: Bonn from +89 degrees to -22 degrees inclusive, Cordoba from -23 degrees to -51 degrees inclusive, Cape Photographic from -52 degrees to -89 degrees inclusive. When a star is not contained in the Durchmusterung proper to its declination zone, but is contained in another Durchmusterung, this is so indicated in the Notes. Other components having different Durchmusterung numbers are also indicated in the Notes ("notesmn.dat"). --- note Notes The following codes are contained in these columns: N: Notes found in the Notes table. O: Orbit. Where motion has exceeded 360 degrees, no values are listed in the position angle and separation columns. Orbits may be found in the "Fourth Catalog of Orbits of Visual Binary Stars" (Worley and Heintz, 1983), and in the Information Circulars published by Commission 26 of the IAU, as well as in the literature. P: 100 year proper motion in right ascension. Q: 100 year proper motion in declination. R: 100 year proper motion in right ascension and declination. a: Pair appears in an appendix list, not part of the discoverer's regular numbering system. r: Pair was listed, but in a "rejected" list, not part of the discoverer's regular numbering sequence. s: Pair has other discoverer's designations and numbers in the literature due to duplicate discovery. We have given credit to the earliest discovery observation (and correct identification) reported in the literature. The List of Synonyms follows the List of Additional Discoverers. p: Coordinates and proper motions from the ACRS, PPM, IRS, and FK5 catalogs. 6: Separation given in minutes of arc rather than se- conds. --- Notes to the WDS Notes (synonyms) to the WDS RAh Right Ascension 2000 (hours) The positions given represent our best estimates of these values. Where possible, these are based on the ACRS and PPM data, with proper motion incorporated. There may be several lines per system, see Cont h RAm Right Ascension 2000 (minutes) min DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DiscName Discoverer Code & Number The discoverer, identified by a one-to-three letter code (see wdsref.dat and wdsrefa.dat for the meaning), and the discoverer's number, if assigned. The reference list ("wdsref.dat") should be consulted first to identify individuals. However, some discoverer designations do not appear in this list, for various reasons, and a supplementary list is provided ("wdsrefa.dat"). --- Cont Continuation flag The + indicates that a continuation exists on the next line: only the last line of the comment has this flag set to blank. --- Text Text of Note We have extensively revised the Notes to include much more information on orbital motion and multiplicity (including astrometric, photometric, and spectroscopic), variability, composite spectra, etc. In the case where an orbit exists for a pair, we give the period (P) and the semi-major axis (a) in seconds of arc, plus an indication of the direction of motion. --- Discoverer References Disc Discoverer Code --- RefNo Reference number of publication --- Obs Observer(s) --- Publ Publication reference for measures --- Discoverer Codes (Additional) Disc Discoverer Code --- Obs Observer --- wds.doc WDS Catalog Documentation G. G. Douglass U.S. Naval Observatory 1996 Oct 02 The ADC thanks Dr. Douglass for not only forwarding the Washington Double Star Catalog and the accompanying documentation in good shape but also for forwarding a revised version correcting the few mistakes discovered in the first version. UNKNOWN UNKNOWN * 02-Oct-1996: Catalogue prepared by G.G. Douglass [U.S. Naval Observatory] * 26-Sep-1997: For 5 stars, the erroneous magnitudes were corrected (concerns WDS J04497+1554, J06283+0155, J12500+4708, J19344+0824 and J23126+0241) I_237.xml The General Catalogue of Trigonometric Stellar Parallaxes, Fourth Edition 1238 I/238 Yale Trigonometric Parallaxes, Fourth Edition The General Catalogue of Trigonometric Stellar Parallaxes, Fourth Edition W F Van Altena J T Lee E D Hoffleit Yale University Observatory ??? ??? 1995 1995GCTP..C......0V Parallaxes, trigonometric This is a completely revised and enlarged edition of the General Catalogue of Trigonometric Stellar Parallaxes containing 15,994 parallaxes for 8,112 stars published before the end of 1995. In this Fourth Edition, 1,722 (27%) new stars have been added to those contained in the previous edition by Jenkins (1963). The mode of the parallax accuracy for the newly added stars (0.004" s.e.) is considerably better than in the previous editions (about 0.016"). Approximately 2300 stars are not in the Hipparcos Catalog. The catalog contains equatorial coordinates in the system of the FK4 for 1900, the total proper motion and its position angle, the weighted average absolute parallax and its standard error, the number of parallax observations, quality of interagreement of the different values, the visual magnitude and various cross identifications with other catalogs. Auxiliary information is listed, including UBV photometry, MK spectral types, data on the variability and binary nature of the stars, and miscellaneous information to aid in determining the reliability of the data.
The 1900 equinox has been maintained to avoid assigning yet another star number and avoid potential errors, since the 1900 based numbers have been used in the Notes and elsewhere in the Catalogue. For each star, the printed catalog contains a reference to the source of publication of the individual parallax The relative parallaxes are corrected to absolute parallax using newly computed corrections that are based on an improved model of the Galaxy. In the Introduction to the printed Catalogue, an analysis of the resulting absolute parallaxes has been made to study the accidental and systematic errors of the parallaxes. Those results provide a "system" for the Catalogue which then yields weighted absolute parallaxes for each star. A preliminary version <I/174> of this catalog was previously archived in the Astronomical Data Centers and was included on the first ADC CD-ROM. In this final version the authors have revised the weighting system, and included newly published parallaxes, photometry and spectral types for most of the stars. The weighted mean parallaxes of many stars will be found to differ from those in the preliminary version due to changes in the weighting system, revisions to the default reference star magnitudes and the addition of new parallaxes.
The data file GCTP Catalog number There are nine stars for which no data are given. They were previously misidentified and had no parallaxes available. They have been retained for completeness in the star numbers. These are: 268.00, 1810.10, 1965.00, 2129.10, 3023.00, 3686.10, 4132.00, 4728.00, and 5699.10. There are no entries in the records for these stars except the identifications. --- RAh Right ascension hours (1900.0) h RAm Right ascension minutes (1900.0) min RAs Right ascension seconds (1900.0) The number of significant figures indicates the accuracy of the position. s DE- Declination sign --- DEd Declination degrees (1900.0) deg DEm Declination minutes (1900.0) arcmin DEs Declination seconds (1900.0) arcsec u_RAm : = lower precision position --- Vmag V magnitude or other magnitude The magnitudes of stars with two digits following the decimal point are photoelectric V magnitudes; the remaining magnitudes are lower accuracy visual magnitudes or miscellaneous other types. Details are given in the printed Catalogue. mag n_Vmag P indicates blue passband --- B-V B-V color mag U-B U-B color mag r_Vmag Source code for photometry --- MK Spectral type The MK type is given if it exists. --- r_MK Source code for spectral type --- comp Double star component M indicates photometrically unresolved components --- var Variable star name A number beginning with S is a New Suspected Variable number (cat. <II/140>) --- HR HR number From Hoffleit, E.D. and Warren, W., 1988 revised in the electronic version (see cat. <V/50>) --- supp S=in Hoffleit BSS Cat. <V/36> --- HD HD number and component --- DM DM identification and component B = Bonner Durchmusterung (catalogs <I/119>, <I/122>) C = Cordoba Durchmusterung (catalog <I/114>) P = Cape Photographic Durchmusterung (catalog <I/108>) --- name Star name --- pm Total Proper motion arcsec/a pmPA Proper motion position angle deg pi Weighted absolute parallax arcsec e_pi Standard error of parallax 0.1marcsec q_pi Quality of interagreement G = good F = fair P = poor X = discordant --- o_pi Number of parallax observations Number of parallax observations included in the weighted average parallax --- Explanation of the source codes type type of source --- code Code for source --- source Source --- Nancy Grace Roman ADC/SSDOO 1996 Nov 14 We thank Dr. Van Altena for sending us the electronic version of the catalog and thank, particularly, Dr. John T. Lee for extensive help in providing the necessary additional information. I_238.xml A normal system of positions and proper motions in the equatorial zone centred at epoch 1970. 1241 I/241 The N70E catalogue A normal system of positions and proper motions in the equatorial zone centred at epoch 1970. Y B Kolesnik Mon. Not. R. Astron. Soc. 285 1 1997 1997MNRAS.285....1K I/80 : Catalog of 5268 Standard Stars, Normal System N30 (Morgan 1952) I/113 : General Catalogue of 33342 stars (GC) (Boss 1937) I/143 : FK4 and FK4 Supplement (Fricke+ 1963) I/149 : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) - Extension (Fricke+ 1991) Fricke, W., Schwan, H., & Lederle, T. (in collaboration with Bastian, U., Bien, R., Burkhardt, G., du Mont, B., Hering, R., Jaehrling, R., Jahreiss, H., Roeser, S., Schwerdtfeger, H. M., & Walter, H. G.) 1988, Fifth Fundamental Catalogue (FK5), Part I. The Basic Fundamental Stars, Veroeff. Astron. Rechen-Institut Heidelb. No. 32 (Catalog <I/149>) Proper motions Positional data catalogs astrometry reference systems The N70E catalogue provides improved mean positions and proper motions for the 718 Basic fundamental stars from the FK5 catalogue in the equatorial zone covering the declination range from -30 to +30 degrees. The catalogue is resulted from revision of the FK5 system on the basis of 36 modern absolute and quasi-absolute catalogues and the four fundamental catalogues FK3, FK4, GC, N30, and revision of FK5 individual positions and proper motions by use of 52 catalogues distributed at the time span from 1900 to 1993. Absolute orientation in space of N70E catalogue is defined by the IAU (1976) system of astronomical constants. Only the machine-readable version of the N70E catalogue is distributed. It contains the positions and proper motions of the stars for the epoch and equinox J2000.0, the mean epochs of individual observed right ascensions and declinations used to determine the final positions, and the mean errors of the final positions and proper motions for the reported epochs.
*The N70E catalogue FK5 FK5 number --- RAh Right ascension hours (J2000.0) h RAm Right ascension minutes (J2000.0) min RAs Right ascension seconds (J2000.0) s pmRA Centennial proper motion in RA (J2000.0) 0.01s/yr DE- Sign of declination (Dec) (J2000.0) --- DEd Declination degrees (J2000.0) deg DEm Declination arcminutes (J2000.0) arcmin DEs Declination arcseconds (J2000.0) arcsec pmDE Proper motion in DE (J2000.0) 0.01arcsec/yr EpRA-1900 Mean Epoch of individual observed RA Mean epoch (-1900.0) of the individual observed right ascensions and declinations as resulted from weighted random improvement of the FK5 positions. yr e_RAs Mean error in individual observed RA The mean errors of the positions at the mean epoch and of the corresponding proper-motion components, as obtained from the solution of the normal equations within the derivations of individual positions and proper motions. It should be emphasised that, by contrast to conventional form of publication of catalogues which belong to FK series, the errors in RAs and pmRA are given in arcseconds, not in seconds of time. (These mean errors do not include those of the N70E system which are estimated about 2 times smaller, see the source reference. It should be noted that the absolute orientation in space of N70E catalogue has been kept from the FK5 system, therefore the errors of FK5 equinox and equator and their secular variations are intrinsically embedded into N70E coordinates.) 0.01arcsec e_pmRA Mean error in individual observed pmRA 0.1mas/yr EpDE-1900 Mean Epoch of individual observed DE yr e_DEs Mean error in individual observed DE 0.01arcsec e_pmDE Mean error in individual observed pmDE 0.1mas/yr Yuri Kolesnik Inst. Astronomy Moscow 1997 Mar 28 Institute of Astronomy of the Russian Academy of Sciences 48 Piatnitskaya St. 109017 Moscow, Russia kolesnik@inasan.rssi.ru I_241.xml The Pulkovo PVC96 catalogue: the first version of catalogue of FK5 stellar declinations observed in 1987-1994 with the Photographic vertical circle. 1242 I/242 Pulkovo Photographic Vertical Circle The Pulkovo PVC96 catalogue: the first version of catalogue of FK5 stellar declinations observed in 1987-1994 with the Photographic vertical circle. A G Gontcharov B K Bagildinsky E V Kornilov D D Polojentsev V D Shkutov Bull. Inf. CDS 49 in press ??? ??? 1997 1997BICDS..49press. I/149 : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) - Extension (Fricke+ 1991) Positional data Meridian observations The Pulkovo photographic vertical circle catalogue, the first version, PVC96, gives accurate declinations of 760 stars from the FK5 and FK5 Extension north of declination -15deg. In 1987-1995 the Photographic vertical circle of the Pulkovo observatory (PVC) carried out programme of observations of declinations of Mars, Jupiter and FK5 stars. Stars with declination higher than 45 deg were observed at both culminations. 8250 observations of 1345 stars and 49 ones of 2 planets have been treated and used to establish an instrumental coordinate frame conform to the DE200. The first version of the catalogue, PVC96, has been constructed on the basis of 6821 observations of 760 stars with at least 4 observations at upper culmination. For the stars with declination higher than 70 deg the observations at both culminations were used in the catalogue, for the rest of the stars only observations at upper culmination were used. The mean observational epoch is 1991.5. The internal mean error of one observation at zenith is 0.14 arcsec. The declinations of the stars are obtained with mean precision of 0.07 arcsec. The classical method of observations with vertical circle was used. Each meridian transit observation includes two exposures of 40 seconds each separated by a reversal of the entire instrument taking about one minute. During the period of the observations the PVC had a photographic-photoelectric micrometer including a photographic camera at the eyepiece end of the tube, and a special visual-photoelectric measuring machine. Readings of two divided vertical circles of glass were registered by photoelectric microscopes. A tilt of the instrument with respect to the vertical line was measured by two bubble levels. All the measuring devices of the PVC were calibrated and investigated externally (i.e., independently of observations). The flexure of the tube investigated at various zenith distances proves to be a function of zenith distance and temperature. The meteorological equipment was calibrated and the temperature, pressure and humidity were read to take refraction into account with a precision of 0.02 arcsec using the Pulkovo Tables, 5th edition. Since narrow red filters were used in the observations, the chromatic refraction was taken from the Pulkovo Tables also. All systematic errors (i.e., those depending on zenith distance) have been evaluated and taken into account with a precision at the level of 0.05 arcsec. Therefore the asymptotic accuracy of the observed declination after many observations has been evaluated as a function of zenith distance. Combining this asymptotic accuracy with formal precision of the obtained declination we evaluated the accuracy for every catalogue declination. The result of the stellar observations is an independent instrumental coordinate frame. Using the planetary observations this instrumental frame is rotated to conform to the DE200 ephemerides which are generally accepted as the best current conventional dynamical frame. It is done by solving for a correction to the equator zero-point derived from the observations of the planets made in the instrumental frame. The corrections to equator are: "instrumental frame minus FK5" (from stellar observations) = +0.014 +/-0.02 arcsec, "instrumental frame minus DE200" (from planetary observations) = -0.046 +/-0.03 arcsec, "catalogue PVC96 minus FK5" = +0.060 +/-0.04 arcsec.
The catalog FK5 Number from FK5 --- HIC Number from Hipparcos Input Catalogue <I/196> --- Nobs Number of observations --- Ep-1900 Mean epoch of observation (years), offset 1900 yr DEdeg Declination (degrees), equinox=J2000, epoch of observation deg PVC96-FK5 Difference between observed and FK5 declination (hundredths of arcseconds), equinox=J2000, epoch of observation 10mas fpDEdeg Formal precision of declination (hundredths of arcseconds) 10mas e_DEdeg Evaluated accuracy of declination (hundredths of arcseconds) 10mas RAh Right ascension from FK5 (hours), equinox=J2000, equator=J2000 h George Gontcharov Pulkovo Obs Francois Ochsenbein CDS 1996 Oct 07 We dedicate the catalogue to the memory of Dr. Bronislav K. Bagildinsky. During more than 30 years he provided important guidance in all works with the Pulkovo photographic vertical circle. On September 26th of this year Dr. Bagildinsky died. He was 67. His scientific contributions, enthusiasm for astrometry, and, most of all, his friendship will be exceedingly missed. The authors thank all astronomers from the Pulkovo observatory who took part in this research: Dr. V.A.Naumov, E.N.Bystrov, M.S.Chubey, Dr. A.V.Devyatkin, Dr. I.S.Guseva, O.M.Mikhailova, Dr. N.R.Persiyaninova, Z.A.Razvorotneva, B.N.Smirnov, E.N.Titova and others, with special thanks to Dr. Anna Andronova for discussion of software and mathematical methods. G.A.G. is grateful to the American Astronomical Society for financial support. The calculations are performed with two computers provided by the Russian foundation of fundamental investigations (grant # 93-02-3056). I_242.xml The Optical Gravitational Lensing Experiment (OGLE). The General Catalog of Stars in the Galactic Bulge. I. Stars in the Central Baade's Window OGLE Field BWC. 1244 I/244 OGLE General Catalog of Stars. I. The Optical Gravitational Lensing Experiment (OGLE). The General Catalog of Stars in the Galactic Bulge. I. Stars in the Central Baade's Window OGLE Field BWC. M Szymanski A Udalski M Kubiak J Kaluzny M Mateo W Krzeminski Acta Astron. 46 1 1996 1996AcA....46....1S II/213 : OGLE Galactic Bulge periodic variables (Udalski+ 1996) J/A+AS/125/343 : RR Lyr stars in omega Cen (Kaluzny+ 1997) Stars, faint Positional data Photometry, CCD catalogs stars: general This paper present the first part of the Optical Gravitational Lensing Experiment (OGLE) General Catalog of Stars in the Galactic Bulge. The catalog is based on observations collected during the OGLE microlensing search. This part contains 33196 stars brighter than I=18mag identified in the Baade's Window BWC field. Stars from remaining 20 OGLE fields will be presented in similar form in the next parts of the Catalog.
Baade's Window Catalog data OGLE Star number (always starting by BWC) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Imag I mean magnitude mag SigI Standard deviation of good I band measurements mag e_Imag rms uncertainty on Imag of a single good measurement mag V-I V-I colour index estimat, if available mag o_Imag Number of good photometry points --- Rem Remarks, including references to the OGLE catalog of Periodic Variables and microlensing candidates --- Patricia Bauer CDS 1997 Apr 25 UNKNOWN UNKNOWN Copied in April 1997 from ftp://sirius.astrouw.edu.pl/ogle//general_catalog/bwc.cat I_244.xml The ACT Reference Catalog 1246 I/246 The ACT Reference Catalog The ACT Reference Catalog S E Urban T E Corbin G L Wycoff Bull. American Astron. Soc., 191, #57.07 ??? ??? 1997 1997AAS...191.5707U I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) The Hipparcos and Tycho Catalogues, 1997, European Space Agency, SP 1200 New Reductions of the Astrographic Catalogue: Plate Adjustments of the Algiers, Oxford I and II, and Vatican Zones, Urban, S.E, Martin, J.C., Jackson, E.S., and Corbin, T.E. =1996A&AS..118..163U New Reductions of the Astrographic Catalogue: Conventional Plate Adjustment of the Cape Zone, Urban S.E. and Corbin T.E. =1996A&A...305..989U The U.S. Naval Observatory Astrographic Catalog Project, Urban, S.E. and Corbin, T.E., Galactic and Solar System Optical Astrometry, ed. Morrison and Gilmore, Camb. Univ. Press, p. 11, 1994 Positional data Proper motions Astrographic zones Historical catalog Photographic catalog Surveys Cross identifications The U.S. Naval Observatory has completed the compilation of the ACT Reference Catalog, containing 988,758 stars covering the entire sky. The motivation behind the ACT was to provide accurate proper motions for the majority of the stars in the Tycho Catalogue (ESA SP-1200). To do this, positions from new reductions of the Astrographic Catalogue (AC 2000) were combined with those of Tycho. The large epoch span between the two catalogs yields proper motions about an order of magnitude more accurate than those published in the Tycho Catalogue. The astrometric data contained in the ACT Reference Catalog include positions, proper motions and error estimates. These are on the Hipparcos System (J2000.0) for epoch J2000.0. Photometric data (B and V) from Tycho are included. Additionally, cross references to the Tycho, AC 2000, Bonner Durchmusterung (BD), Cordoba Durchmusterung (CD), Cape Durchmusterung (CPD), Henry Draper (HD) and Hipparcos Catalogues are given.
ACT Reference Catalog [00h 00m - 00h 30m[ ACT Reference Catalog [00h 30m - 01h 00m[ ACT Reference Catalog [01h 00m - 01h 30m[ ACT Reference Catalog [01h 30m - 02h 00m[ ACT Reference Catalog [02h 00m - 02h 30m[ ACT Reference Catalog [02h 30m - 03h 00m[ ACT Reference Catalog [03h 00m - 03h 30m[ ACT Reference Catalog [03h 30m - 04h 00m[ ACT Reference Catalog [04h 00m - 04h 30m[ ACT Reference Catalog [04h 30m - 04h 00m[ ACT Reference Catalog [05h 00m - 05h 30m[ ACT Reference Catalog [05h 30m - 06h 00m[ ACT Reference Catalog [06h 00m - 06h 30m[ ACT Reference Catalog [06h 30m - 07h 00m[ ACT Reference Catalog [07h 00m - 07h 30m[ ACT Reference Catalog [07h 30m - 08h 00m[ ACT Reference Catalog [08h 00m - 08h 30m[ ACT Reference Catalog [08h 30m - 09h 00m[ ACT Reference Catalog [09h 00m - 09h 30m[ ACT Reference Catalog [09h 30m - 10h 00m[ ACT Reference Catalog [10h 00m - 10h 30m[ ACT Reference Catalog [10h 30m - 11h 00m[ ACT Reference Catalog [11h 00m - 11h 30m[ ACT Reference Catalog [11h 30m - 12h 00m[ ACT Reference Catalog [12h 00m - 12h 30m[ ACT Reference Catalog [12h 30m - 13h 00m[ ACT Reference Catalog [13h 00m - 13h 30m[ ACT Reference Catalog [13h 30m - 14h 00m[ ACT Reference Catalog [14h 00m - 14h 30m[ ACT Reference Catalog [14h 30m - 15h 00m[ ACT Reference Catalog [15h 00m - 15h 30m[ ACT Reference Catalog [15h 30m - 16h 00m[ ACT Reference Catalog [16h 00m - 16h 30m[ ACT Reference Catalog [16h 30m - 17h 00m[ ACT Reference Catalog [17h 00m - 17h 30m[ ACT Reference Catalog [17h 30m - 18h 00m[ ACT Reference Catalog [18h 00m - 18h 30m[ ACT Reference Catalog [18h 30m - 19h 00m[ ACT Reference Catalog [19h 00m - 19h 30m[ ACT Reference Catalog [19h 30m - 20h 00m[ ACT Reference Catalog [20h 00m - 20h 30m[ ACT Reference Catalog [20h 30m - 21h 00m[ ACT Reference Catalog [21h 00m - 21h 30m[ ACT Reference Catalog [21h 30m - 22h 00m[ ACT Reference Catalog [22h 00m - 22h 30m[ ACT Reference Catalog [22h 30m - 23h 00m[ ACT Reference Catalog [23h 00m - 23h 30m[ ACT Reference Catalog [23h 30m - 24h 00m[ RAh Right Ascension ICRS, Eq=J2000 (hours) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed h RAm Right Ascension ICRS (minutes) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed min RAs Right Ascension ICRS (seconds) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed s DE- Declination ICRS, Epoch=J2000.0 (sign) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- DEd Declination ICRS, Epoch=J2000.0 (degrees) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed deg DEm Declination ICRS (minutes) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed arcmin DEs Declination ICRS (seconds) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed arcsec pmRA Proper Motion in RA, (sec of time/yr) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed s/yr pmDE Proper Motion in Dec, arcsec/yr) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed arcsec/yr e_RAs Stand. dev. of RA at Epoch 1991.25 from Tycho (T14) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed mas e_DEs Stand. dev. of Dec at Epoch 1991.25 from Tycho (T15) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed mas e_pmRA Stand. dev. of Proper motion (RA), number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed mas/yr e_pmDE Stand. dev. of Proper motion (DE), number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed mas/yr BTmag Blue magnitude from Tycho (T32) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed mag VTmag Visual magnitude from Tycho (T34) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed mag B-V Johnson B-V from Tycho (T37) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed mag flag1 Astrometric Quality flag (T10) Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- flag2 Quality flag (T40) Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- flag3 Known variability flag (T47) Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- flag4 Variability from Tycho (T48) Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- flag5 Duplicity from Tycho (T49) Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- TYC Tycho ID, embedded zeros for blanks number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- AC2000 AC 2000 Number number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- BD BD identifier (T54) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- CD CD identifier (T55) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- CPD CPD identifier (T56) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- HD Henry Draper Number (T53) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- HIP Hipparcos Number (T31) number= Astrometry Flag (T10 in Tycho): blank: a recommended astrometric reference star X: a dubious astrometric reference star in Tycho number= Quality flag (T40 in Tycho): 1 through 5: very high to medium quality; probably single stars 6: perhaps non-single 7: low astrometric quality 8: perhaps non-stellar blank: unassigned, observed by Hipparcos, not Tycho number= Known variability flag (T47 in Tycho) G: Star in General Catalogue of Variable Stars, 4th Edition N: Star in New Catalogue of Suspected Variable Stars number= Variability from Tycho (T48 in Tycho) U: Apparent variability in Tycho data; may be due to duplicity V: strong evidence of variability in the Tycho data W: variability suspected in the Tycho data number= Duplicity from Tycho (T49 in Tycho) Y: Investigation of duplicity made, no indication of duplicity Z: No investigation of duplicity was performed --- intro.tex Introduction, latex version intro.ps Introduction, postscript version Sean E. Urban U.S. Naval Observatory 1997 Sep 04 I_246.xml The AC2000: the Astrographic Catalogue on the Hipparcos System 1247 I/247 The AC2000 Catalogue The AC2000: the Astrographic Catalogue on the Hipparcos System S E Urban T E Corbin G L Wycoff US Naval Observatory ??? ??? 1997 1997 I/171 : Astrographic Catalog Reference Stars (ACRS) (Corbin+ 1991) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) I/246 : The ACT Reference Catalog (Urban+ 1997) http://aries.usno.navy.mil/ad/ac.html : AC web site Positional data Astrographic zones Surveys The Astrographic Catalogue (AC) was an international effort designed to photograph and measure the positions of all stars brighter than magnitude 11.0. In total, some 4.6 million stars were observed, many as faint as 13th magnitude. Users should realize that a few thousand of the brightest stars are not included; their images on the source plates were grossly over-exposed and therefore measurements were often not made. This project was started over 100 years ago, and the positions that have been derived from the AC data are being used, in combination with modern epoch positions, to determine accurate proper motions. The United States Naval Observatory has completed the reductions of the Astrographic Catalogue data (AC) to a consistent system. The resulting catalog, called AC 2000, contains 4,621,836 stars covering the entire sky, at an average epoch of 1907. The positions are on the Hipparcos reference frame (J2000.0) at the epochs of observation. Each of the 22 zones making up the Astrographic Catalogue was reduced independently using the Astrographic Catalog Reference Stars (ACRS). Each was analyzed for tilt, radial and tangential distortions, coma, magnitude equation and non-symmetric field distortions. Following these reductions, the data were placed on the Hipparcos system and the magnitudes were converted to be close to that of the Tycho B data. The resulting data were then combined into the final catalog. Detailed information on the reduction methodology and input data can be found in the file "intro.tex", or in the postscript documents provided provided in the "ps" subdirectory. The data contain the positions (eq. J2000.0) at mean epochs of observation, magnitude estimates and accuracy estimates for each star. Cross identifications with the Hipparcos Catalogue, Tycho Catalogue and the Astrographic Catalog Reference Stars are provided to facilitate future work with these stars. Interested parties are encouraged to visit the AC web site at http://aries.usno.navy.mil/ad/ac/ac.html
Stars with declinations +60 to +90 degrees Stars with declinations +50 to +59 59 59.99 Stars with declinations +40 to +49 59 59.99 Stars with declinations +30 to +39 59 59.99 Stars with declinations +20 to +29 59 59.99 Stars with declinations +10 to +19 59 59.99 Stars with declinations +00 to +09 59 59.99 Stars with declinations -00 to -09 59 59.99 Stars with declinations -10 to -19 59 59.99 Stars with declinations -20 to -29 59 59.99 Stars with declinations -30 to -39 59 59.99 Stars with declinations -40 to -49 59 59.99 Stars with declinations -50 to -59 59 59.99 Stars with declinations -60 to -90 degrees RAh Right Ascension (ICRS) at Epoch (hours) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. h RAm Right Ascension (ICRS) at Epoch (minutes) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. min RAs Right Ascension (ICRS) at Epoch (seconds) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. s DE- Declination (ICRS) at Epoch (sign) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. --- DEd Declination (ICRS) at Epoch (degrees) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. deg DEm Declination (ICRS) at Epoch (minutes) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. arcmin DEs Declination (ICRS) at Epoch (seconds) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. arcsec Bmag Magnitude from image diameters number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. mag Epoch Mean epoch of position number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. yr Num Number of images used number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. --- e_RAs Standard deviation of mean, RA number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. arcsec e_DEs Standard deviation of mean, Dec number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. arcsec AC2000 AC 2000 Number number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. --- HIP Hipparcos Number (Cat. <I/239>) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. --- TYC Tycho ID (Cat. <I/239>) Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. --- ACRS ACRS number (Cat. <I/171>) number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. --- Vflag Verification Flag The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. number= Tycho "number" originally had embedded blanks. These embedded blanks have been converted to zeros. number= The Verification flag is either blank or '1'. When set to '1', the star has not been found in Hipparcos, Tycho, ACRS, the overlapping AC plate or in the GSC 1.2. These records should be used with caution. --- intro.tex Original Introduction (latex) Sean E. Urban U.S. Naval Observatory 1998 Nov 10 Reductions by the Astrometry Department U.S. Naval Observatory 3450 Massachusetts Ave. NW Washington, DC 20392-5420 e-mail: seu@pyxis.usno.navy.mil UNKNOWN UNKNOWN The data are a copy of the CD-ROM "The AC 2000 Catalog" from U.S. Naval Observatory, September 1997. UNKNOWN UNKNOWN Usage Notice: Any use of the data in publication must be accompanied by a citation as to the original author. I_247.xml The Tokyo PMC Catalog 90-93: Catalog of Positions of 6649 Stars Observed in 1990 through 1993 with Tokyo Photoelectric Meridian Circle 1248 I/248 Tokyo Photoelectric Meridian Circle Catalog 90-93 The Tokyo PMC Catalog 90-93: Catalog of Positions of 6649 Stars Observed in 1990 through 1993 with Tokyo Photoelectric Meridian Circle M Yoshizawa S Suzuki Publ. Nat. Astron. Obs. Japan 5 1 1997 1997PNAOJ...5....1Y I/186 : Tokyo PMC Catalog 85 (Yoshizawa+ 1987) I/167 : Tokyo PMC Catalog 86 (Yoshizawa+ 1989) I/187 : Tokyo PMC Catalog 87 (Yoshizawa+ 1991) I/188 : Tokyo PMC Catalog 88 (Yoshizawa+ 1992) I/198 : Tokyo PMC Catalog 89 (Yoshizawa+ 1993) Yasuda,H., Furukawa,K. and Hara,H.: 1982, Ann. Tokyo Astron. Obs., 2nd Ser., 18, 367-427 Yasuda,H., Hara,H., Fukaya,R. and Ishii,H.: 1986, Ann. Tokyo Astron. Obs., 2nd Ser., 21, 107-126 (1986AnTok..21..107Y) Meridian observations Positional data The sixth annual catalog of the Tokyo PMC is presented for 6649 stars which were observed at least two times in January 1990 through March 1993. The mean positions of the stars observed in the above period are given in the catalog at the corresponding mean epochs of observations of individual stars. The coordinates of the catalog are based on the FK5 system, and referred to the equinox and equator of J2000.0. The mean local deviations of the observed positions from the FK5 catalog positions are constructed for the basic FK5 stars to compare with those of the Tokyo PMC Catalog 89 and preliminary Hipparcos results of H30. The catalog contains the positions of 1180 basic FK5 stars, 322 FK4 Suppl. stars, 3132 AGK3R stars, 141 OB stars, 252 NPZT stars, and 1601 SAO stars observed with the Tokyo Photoelectric Meridian Circle in the 1990 to 1993 periods based on the FK5 system. The positions of the stars are given for the mean epoch of the observations of individual stars referring to the equinox and equator of J2000.0. The values of (O-C)s in the catalog are calculated by using the positions given in the source catalog, and by evaluating those at the mean epoch of observations of each star, with the equinox and equator at the mean epoch. The magnitudes of the stars given in the catalog can be transformed into the V-magnitude of the standard UBV system by the equation : V = V(TPMC) + 0.063(B-V) - 0.045.
The catalog N sequence number in the Catalog --- Cat other catalogue name number=1 Besides obvious standard designations, AGK3 : star numbers are composed as DDNNNN, H2O : Unpublished list of H2O masers and related objects; star numbers are preliminary number in an observing list, OB : "Catalog of O-B Stars Observed with Tokyo Meridian Circle" (Yasuda+ 1986), N.B.: star numbers are not the catalog numbers but the OBSNO's deducted by 15000 (OBSNO: preliminary star number in an observing program), PZT : "Northern PZT Star Catalog" (Yasuda+ 1982), N.B.: star numbers are not the catalog numbers but the OBSNO's, which are preliminary star numbers in the Northern PZT Star list. --- otherN star number in other catalogues --- otherMag visual magnitude in other catalogues mag Sp spectral type --- Ep-1900 mean epoch of the observations of R.A. and Dec (offset 1900) a Nobs number of observations of R.A. and Dec. --- RAh observed J2000 R.A. at the mean epoch (hours) h RAm observed R.A. at the mean epoch (minutes) min RAs observed R.A. at the mean epoch (seconds) s DE- observed J2000 Dec. at the mean epoch (sign) --- DEd observed Dec. at the mean epoch (degrees) deg DEm observed Dec. at the mean epoch (minutes) arcmin DEs observed Dec. at the mean epoch (seconds) arcsec O-C_RA (O-C) in R.A. at the mean epoch to be added to the Source Catalogue s O-C_DE (O-C) in Dec. at the mean epoch to be added to the Source Catalogue arcsec e_RAs mean error of the observed R.A. s e_DEs mean error of the observed Dec. arcsec EpMag-1900 mean epoch of the observations of magnitude a o_Mag number of observations of magnitude --- Mag observed magnitude at the mean epoch mag e_Mag mean error of the observed magnitude mag DM DM numbers number=2 BD number for Dec. > -23 degrees, and CD number for Dec. < -23 degrees, component designations "p, s, x" are those used in PPM catalogues (<I/146>, <I/193>, <I/208>) --- AGK AGK3 numbers number=3 An asterisk at byte 134 indicates that the entry is an unresolved double star which has two AGK3 numbers, i.e. "+41 1873" and "+41 1874". --- S.Nishimura ADAC/NAOJ 1998 Apr 08 I_248.xml Catalog of O-B stars observed with Tokyo meridian circle 1249 I/249 Tokyo meridian circle catalog of O-B stars Catalog of O-B stars observed with Tokyo meridian circle H Yasuda H Hara R Fukaya H Ishii Ann. Tokyo Astron. Obs. 21 107 1986 1986AnTok..21..107Y I/143 : FK4 and FK4 supplement V/31 : Kinematic data for O-B5 stars (Rubin+, 1962) Blaauw, 1953 IAU Symposium No. 1, "Coordination of Galactic Researches" Meridian observations Stars, OB A catalog of the O-B stars, selected from "Blaauw-Parenago" list (1955, First IAU Symposium, "Co-ordination of galactic research") and Rubin's catalog (1962AJ.....67..491R, Cat. <V/31>), has been compiled on the FK4 system by the observations made with Gautier 8-inch Meridian Circle at the Tokyo Astronomical Observatory during the period, 1971 to 1979. It contains 1059 stars and was compiled for the future establishment of high precision proper motions of O-B stars.
Catalog of O-B stars observed with Tokyo meridian circle Seq Catalog Number --- Vmag Visual Magnitude mag SpType Spectral Type --- RAh Right Ascension (1950, EpRA-1900) number=1 The positions are referred to the equinox and equator of 1950.0 in the FK4 system and reduced to the epoch of observation. h RAm Right Ascension (1950, EpRA-1900) number=1 The positions are referred to the equinox and equator of 1950.0 in the FK4 system and reduced to the epoch of observation. min RAs Right Ascension (1950, EpRA-1900) number=1 The positions are referred to the equinox and equator of 1950.0 in the FK4 system and reduced to the epoch of observation. s e_RAs Mean error of catalog position s EpRA-1900 Epoch of observation, 1900.0+ yr o_RAh Number of observations in RA --- pmRA Centurial proper motion in RA number=2 Centurial proper motions used in the computations of reductions of observations 0.01s/yr DE- Declination sign --- DEd Declination (1950, EpochDE) number=1 The positions are referred to the equinox and equator of 1950.0 in the FK4 system and reduced to the epoch of observation. deg DEm Declination (1950, EpochDE) number=1 The positions are referred to the equinox and equator of 1950.0 in the FK4 system and reduced to the epoch of observation. arcmin DEs Declination (1950, EpochDE) number=1 The positions are referred to the equinox and equator of 1950.0 in the FK4 system and reduced to the epoch of observation. arcsec e_DEs Mean Error of Catalog Position arcsec EpDE-1900 Epoch of observation, 1900.0+ yr o_DEd Number of observations in declination. --- pmDE Centurial proper motion in declination number=2 Centurial proper motions used in the computations of reductions of observations 10mas/yr No Preliminary star number in an observing program --- BD BD (Cat. <I/122>) number --- James Marcout, Patricia Bauer CDS 1997 Mar 18 UNKNOWN UNKNOWN Prepared via OCR at CDS. I_249.xml The Tycho Reference Catalogue 1250 I/250 The Tycho Reference Catalogue The Tycho Reference Catalogue E Hog A Kuzmin U Bastian C Fabricius K Kuimov L Lindegren V V Makarov S Roeser Astron. Astrophys. 335L, 65 ??? ??? 1998 1998A&A...335L..65H I/220 : The HST Guide Star Catalog (Lasker+ 1992) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) I/246 : The ACT Reference Catalog (Urban+ 1997) Positional data Proper motions Astrographic zones Historical catalog Photographic catalog Surveys Cross identifications astrometry reference catalogs proper motions Astrographic Catalogue Tycho Catalogue The Tycho Reference Catalogue (TRC) contains high-quality positions and proper motions for 990182 stars of the Tycho Catalogue. The proper motions were derived from Tycho positions and Astrographic Catalogue positions reduced to the Hipparcos system. The median accuracy of the TRC position components is 40 mas at J1991.25. The median accuracy of the proper motion is about 2.5 mas/yr. Systematic errors are less than about 1.0 mas(/yr). The quality of the proper motions in TRC is assessed by comparison with the Hipparcos and Tycho Catalogues. Comparison with the recent ACT Catalogue which is based on an independent reduction of the same observations as used for constructing the TRC is reported.
Hipparcos
The TRC catalogue TYCID1 TYCID1 from TYC number=1 The TYCID1 is the GSC region number, the TYCID2 is the running number within the region, the TYCID3 is a component identifier (normally 1). Some non-GSC running numbers were constructed for TYC. The recommended star designation contains a hyphen between the TYCID numbers, e.g. TYC 1-13-1. --- TYCID2 TYCID2 from TYC number=1 The TYCID1 is the GSC region number, the TYCID2 is the running number within the region, the TYCID3 is a component identifier (normally 1). Some non-GSC running numbers were constructed for TYC. The recommended star designation contains a hyphen between the TYCID numbers, e.g. TYC 1-13-1. --- TYCID3 TYCID3 from TYC number=1 The TYCID1 is the GSC region number, the TYCID2 is the running number within the region, the TYCID3 is a component identifier (normally 1). Some non-GSC running numbers were constructed for TYC. The recommended star designation contains a hyphen between the TYCID numbers, e.g. TYC 1-13-1. --- RAdeg Right Ascension, ICRS, at epoch J2000 deg DEdeg Declination, ICRS, at epoch J2000 deg pmRA prop. mot. in RA * cos(dec) mas/a pmDE proper motion in Dec mas/a epRA mean epoch of RA number=2 The mean epochs are given in Julian years. a epDE mean epoch of Dec number=2 The mean epochs are given in Julian years. a e_RAdeg s.e. RA * cos(dec), at mean epoch number=3 The standard errors given are for the mean epoch. They are in the range 1.0-117.1. The standard errors at some epoch, t, are obtained as e_RA(t)* = sqrt((f*e_RA*)^2^ + ((e_pmRA*)*(t-epRA))^2^ ) and e_DE(t) = sqrt((f*e_DE)^2^ + (e_pmDE*(t-epRA))^2^ ) A factor f=1.5 would give realistic standard errors for the majority of stars. This factor compensates for too small formal errors of positions in the Tycho Catalogue (Cf. Sect 18.4 of Vol 4 of "The Hipparcos and Tycho Catalogues", ESA SP-1200, 1997). mas e_DEdeg s.e. of Dec at mean epoch number=3 The standard errors given are for the mean epoch. They are in the range 1.0-117.1. The standard errors at some epoch, t, are obtained as e_RA(t)* = sqrt((f*e_RA*)^2^ + ((e_pmRA*)*(t-epRA))^2^ ) and e_DE(t) = sqrt((f*e_DE)^2^ + (e_pmDE*(t-epRA))^2^ ) A factor f=1.5 would give realistic standard errors for the majority of stars. This factor compensates for too small formal errors of positions in the Tycho Catalogue (Cf. Sect 18.4 of Vol 4 of "The Hipparcos and Tycho Catalogues", ESA SP-1200, 1997). mas e_pmRA s.e. prop mot in RA * cos(dec) mas/a e_pmDE s.e. of proper motion in Dec mas/a BT Tycho BT magnitude number=4 The BT and VT photometry is copied from the Tycho Catalogue. Approximate Johnson photometry may be obtained as: V = VT -0.090*(BT-VT) B-V = 0.850*(BT-VT) Consult Sect 1.3 of Vol 1 of "The Hipparcos and Tycho Catalogues", ESA SP-1200, 1997, for details. mag e_BT s.e. of BT number=4 The BT and VT photometry is copied from the Tycho Catalogue. Approximate Johnson photometry may be obtained as: V = VT -0.090*(BT-VT) B-V = 0.850*(BT-VT) Consult Sect 1.3 of Vol 1 of "The Hipparcos and Tycho Catalogues", ESA SP-1200, 1997, for details. mag VT Tycho VT magnitude number=4 The BT and VT photometry is copied from the Tycho Catalogue. Approximate Johnson photometry may be obtained as: V = VT -0.090*(BT-VT) B-V = 0.850*(BT-VT) Consult Sect 1.3 of Vol 1 of "The Hipparcos and Tycho Catalogues", ESA SP-1200, 1997, for details. mag e_VT s.e. of VT number=4 The BT and VT photometry is copied from the Tycho Catalogue. Approximate Johnson photometry may be obtained as: V = VT -0.090*(BT-VT) B-V = 0.850*(BT-VT) Consult Sect 1.3 of Vol 1 of "The Hipparcos and Tycho Catalogues", ESA SP-1200, 1997, for details. mag Num Number of positions used number=5 Between 2 and 13 positions (TYC plus 1-12 AC positions) were used in the adjustment: Npos: 2 3 4 5 6 7 8 9 10 11 12 13 Stars: 20183 588096 312449 47150 18045 3169 742 217 81 33 14 3 --- q_pm quality flag for proper motion number=6 q_pm (0..9) gives twice the ratio of the estimated s.e. to the formal s.e. A large value may be taken as a warning. The value 9 marks proper motions deviating from HIP values by more than six combined standard errors. Separate values were computed for R.A. and Dec. Here the maximum value is given. The quality flag was computed prior to the adjustment of the standard errors (Cf Sect 3 of Hoeg et al. 1998). q_pm: 0 1 2 3 4 5 6 7 8 9 Stars 35082 271197 319970 183564 93971 45973 22662 11459 3494 2810 --- HD HD identifier from TYC --- HIP Hipparcos number from TYC --- CCDM CCDM component identifier from TYC number=7 The CCDM component identifier is only given for HIP stars. It is copied from field T51 of the Tycho Catalogue. --- Plx parallax for HIP stars number=8 The parallax for HIP stars is copied from field H11 of the Hipparcos Catalogue, but only when it exceeds the standard error. The HIP parallax was NOT used in the construction of the TRC. mas dupflg duplicity flag number=9 the duplicity flag is set for 16587 stars where duplicity was clearly indicated or suspected in the Tycho data, but not resolved. (T49 is D or S in TYC). --- varflg variability flag number=10 the variability flag is set for 18505 stars with known variability. (T47 set or T48='V' in TYC). --- ACTflg ACT flag number=11 ' ' = also in ACT, proper motion agrees within 10 mas/yr in both coordinates; 'T' = only in TRC (39892 stars); 'X' = also in ACT, does not agree within 10 mas/yr (19104 stars). --- Index to TRC rec Rec. numb. of 1st star in each region number=1 The catalogue is sorted according to the GSC region numbers. The line i of the index file gives the record number in TRC of the first star in GSC region i. Line i+1 gives the record number +1 of the last star in GSC region i. --- Claus Fabricius Niels Bohr Institute for Astronomy 1998 Apr 03 I_250.xml The Guide Star Catalog Version 1.2 1254 I/254 The HST Guide Star Catalog, Version 1.2 The Guide Star Catalog Version 1.2 B M Lasker J N Russel H Jenkner The Association of Universities for Research in Astronomy, Inc. ([c] 1989 1992 1996 1990AJ.....99.2019L The Guide Star Catalog Version 1.2 B M Lasker C R Sturch B J McLean J L Russell H Jenkner M M Shara Astron. J. 99 2019 1990 1990AJ.....99.2019L The Guide Star Catalog Version 1.2 J L Russell B M Lasker B J McLean C R Sturch H Jenkner Astron. J. 99 2059-2081 1990 1990AJ.....99.2059R The Guide Star Catalog Version 1.2 H Jenkner B M Lasker C R Sturch B J McLean M M Shara J L Russell Astron. J. 99 2082 1990 1990AJ.....99.2082J I/220 : The HST Guide Star Catalog, Version 1.1 (Lasker+ 1992) http://www-gsss.stsci.edu/gsc/gsc.html : GSC pages at STScI http://www-gsss.stsci.edu/gsc/gsc12/description.html : GSC 1.2 page http://www-gsss.stsci.edu/gsc/gsc12/gsc12_form.html : GSC 1.2 access Surveys Positional data The Guide Star Catalog (GSC), which has been constructed to support the operational need of the Hubble Space Telescope contains nearly 19 million objects brighter than sixteenth magnitude, of which more than 15 million are classified as stars. This catalog provides positions and magnitudes for these stars. The original version of this catalog, GSC 1.0, is described in a series of papers: Lasker et al. (1990AJ.....99.2019L); Russell et al. (1990AJ.....99.2059R); and Jenkner et al. (1990AJ.....99.2082J) The reference material for the GSC 1.2 reduction is the "Positions and Proper Motions Catalogue": PPM-North, Roeser S. and Bastian U., 1988, Cat. <I/146> PPM-South, Bastian U. and Roeser S., 1993, Cat. <I/193> PPM-Suppl, Roeser S., Bastian U. and Kuzmin A., 1994, Cat. <I/208> and the Astrographic Catalogue (AC) which was used to remove the mean systematics common to all the plates. The overall rms error of the GSC 1.2 is estimated better than 0.3arcsec The STScI provides the details of the GSC versions ("See also" section below)
Sample output (out of 25,258,765 positions) GSC GSC designation the GSC Identification is made of a plate number (5 digits) and star number on the plate (5 digits); note that, in the literature, a dash separates generally the two parts. --- RAdeg Right ascension in J2000, epoch of plate deg DEdeg Declination in J2000, epoch of plate deg PosErr Mean error on position arcsec Pmag photographic magnitude (see n_Pmag) mag e_Pmag photographic magnitude mag n_Pmag Coded passband for magnitude the number designates the following combination of emulsion and filter: magband emulsion filter Notes ------- -------- -------- ----------------------- 0 IIIaJ GG395 SERC-J/EJ 1 IIaD W12 Pal Quick-V 3 --- B Johnson 4 --- V Johnson 5 IIIaF RG630 Red 6 IIaD GG495 Pal QV/AAO XV 7 103aO --- POSS-I Blue 8 103aE red plex POSS-I Red 10 IIaD GG495 GPO Astrograph 11 103aO GG400 Black Birch Astrograph 16 IIIaJ GG495 QV 18 IIIaJ GG385 POSS-II Blue ------- -------- -------- --- Class Class of object (0=star; 3=non-stellar) --- Plate Plate designation two plates (+056 and +017) represent data from catalogues (mainly Hipparcos Input Catalogue, Cat. <I/196>). They have no associated epoch. --- Epoch Epoch of plate yr Mult True if multiple object / False otherwise --- Brian McLean STScI Francois Ochsenbein CDS 1999 May 08 I_254.xml The Guide Star Catalog Version 1.1-ACT (GSC-ACT Catalogue) 1255 I/255 The HST Guide Star Catalog, Version GSC-ACT The Guide Star Catalog Version 1.1-ACT (GSC-ACT Catalogue) B M Lasker J N Russel H Jenkner The Association of Universities for Research in Astronomy, Inc. ([c] 1989 1992 1996 1990AJ.....99.2019L The Guide Star Catalog Version 1.1-ACT (GSC-ACT Catalogue) B M Lasker C R Sturch B J McLean J L Russell H Jenkner M M Shara Astron. J. 99 2019 1990 1990AJ.....99.2019L The Guide Star Catalog Version 1.1-ACT (GSC-ACT Catalogue) J L Russell B M Lasker B J McLean C R Sturch H Jenkner Astron. J. 99 2059-2081 1990 1990AJ.....99.2059R The Guide Star Catalog Version 1.1-ACT (GSC-ACT Catalogue) H Jenkner B M Lasker C R Sturch B J McLean M M Shara J L Russell Astron. J. 99 2082 1990 1990AJ.....99.2082J I/220 : The HST Guide Star Catalog, Version 1.1 (Lasker+ 1992) I/254 : The HST Guide Star Catalog, Version 1.2 (Lasker+ 1992) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) I/246 : The ACT Reference Catalog (Urban+ 1997) I/250 : The Tycho Reference Catalogue (Hog+ 1998) http://www-gsss.stsci.edu/gsc/gsc.html : GSC pages at STScI http://www.projectpluto.com/gsc_act.htm : GSC-ACT Original Description Surveys Positional data The Guide Star Catalog (GSC), which has been constructed to support the operational need of the Hubble Space Telescope contains nearly 19 million objects brighter than sixteenth magnitude, of which more than 15 million are classified as stars. This catalog provides positions and magnitudes for these stars. The original version of this catalog, GSC 1.0, is described in a series of papers: Lasker et al. (1990AJ.....99.2019L); Russell et al. (1990AJ.....99.2059R); and Jenkner et al. (1990AJ.....99.2082J) The reference material for the GSC 1.2 reduction is the "Positions and Proper Motions Catalogue": PPM-North, Roeser S. and Bastian U., 1988, Cat. <I/146> PPM-South, Bastian U. and Roeser S., 1993, Cat. <I/193> PPM-Suppl, Roeser S., Bastian U. and Kuzmin A., 1994, Cat. <I/208> and the Astrographic Catalogue (AC) which was used to remove the mean systematics common to all the plates. The GSC GSC-ACT is a recalibration of GSC1.1 using the ACT (Astrographic Catalog/Tycho, catalog <I/246>) performed by the Project Pluto ("See also" section below). The "plate RMS" values are given at http://www.projectpluto.com/results.txt, with most plates coming in at under .3 arcseconds
Sample output (out of 25,258,765 positions) GSC GSC designation the GSC Identification is made of a plate number (5 digits) and star number on the plate (5 digits); note that, in the literature, a dash separates generally the two parts. --- RAdeg Right ascension in J2000, epoch of plate deg DEdeg Declination in J2000, epoch of plate deg PosErr Mean error on position arcsec Pmag photographic magnitude (see n_Pmag) mag e_Pmag photographic magnitude mag n_Pmag Coded passband for magnitude the number designates the following combination of emulsion and filter: magband emulsion filter Notes ------- -------- -------- ----------------------- 0 IIIaJ GG395 SERC-J/EJ 1 IIaD W12 Pal Quick-V 3 --- B Johnson 4 --- V Johnson 5 IIIaF RG630 Red 6 IIaD GG495 Pal QV/AAO XV 7 103aO --- POSS-I Blue 8 103aE red plex POSS-I Red 10 IIaD GG495 GPO Astrograph 11 103aO GG400 Black Birch Astrograph 16 IIIaJ GG495 QV 18 IIIaJ GG385 POSS-II Blue ------- -------- -------- --- Class Class of object (0=star; 3=non-stellar) --- Plate Plate designation two plates (+056 and +017) represent data from catalogues (mainly Hipparcos Input Catalogue, Cat. <I/196>). They have no associated epoch. --- Epoch Epoch of plate yr Mult True if multiple object / False otherwise --- Bill Gray Project Pluto Francois Ochsenbein CDS 1999 Sep 15 I_255.xml Two-Micron Sky Survey 2002B II/2B Two-Micron Sky Survey Two-Micron Sky Survey G Neugebauer R B Leighton NASA SP-3047 ??? ??? 1969 1969tmss.book.....N Photometry, infrared Surveys The catalog, giving sources of emission in the 2.2-micrometer region for more than 5000 stars, represents a systematic survey of the Northern Hemisphere for stars brighter than third magnitude. The survey was carried out with a telescope at Mount Wilson, California, having a 62-inch diameter and an f/l aluminized epoxy mirror mounted equatorially. Radiation at an effective wavelength of 2.2 micrometers was detected by a lead sulfide photoconductive cell cooled by liquid nitrogen. In addition to the 2.2-micrometer detector array, radiation at an effective wavelength of 0.84 micrometers was detected by a simple silicon photovoltaic cell. The catalog includes right ascension and declination (B1950.0), K and I magnitudes, number of measurements, V magnitude, spectral types, cross identifications to the numbering systems of the General Catalogue, the Durchmusterung catalogs, the Bright Star Catalogue, and star names.
Catalog Data Catalog Data by RA ID Two-Micron Sky Survey number (TMSS) --- n_ID Remark = 1, if there is a remark; = 0, otherwise --- RAh Right ascension 1950 (hours) h RAm Right ascension 1950 (minutes) min RAs Right ascension 1950 (seconds) s DE- Sign of declination --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (arc minutes) arcmin u_RAs Right ascension 1950 uncertainty --- RAs_X2 Right ascension chi-square s u_DEm Declination 1950 uncertainty --- DEm_X2 Declination chi-square arcmin Kmag K magnitude Ignore if byte 76 = 3 or 4. mag e_Kmag K error (ignore if byte 76 = 3 or 4) mag Kmag_X2 K chi-square Ignore if byte 76 = 3 or 4. mag Imag I magnitude Ignore if I magnitude > 14.0 and/or ignore if byte 76 = 2 or 4. mag e_Imag I error Ignore if I magnitude > 14.0 and/or ignore if byte 73 = 1 and/or ignore if byte 76 = 2 or 4. mag Imag_X2 I chi-square Ignore if I magnitude > 14.0 and/or ignore if byte 73 = 1 and/or ignore if byte 76 = 2 or 4. mag n_Imag I magnitude questionable = 1, if I magnitude is questionable; = 0, otherwise --- KIX2 I and K chi-square excess = 1, if chi-square is not excessive = 2, if I chi-square is excessive = 3, if K chi-square is excessive = 4, if I and K chi-square are excessive --- n_KIX2 I and K scale = 1, if I and K both on scale = 2, if I off scale = 3, if K off scale = 4 if both I and K off scale --- ct_Kmag Number of K measurements ct ct_Imag Number of I measurements ct n_ctmag Remark on K and I counts = 1, if there is a remark; = 0, otherwise --- obs_dates Observational timetable Range of days on which observations were made starting with January 30, 1965, and running through April 7, 1968. d Vmag V magnitude mag SpType Spectral type --- Lum Luminosity class = 2, luminosity class I and II = 3, luminosity class III = 4, luminosity class IV = 5, luminosity class V = 6, luminosity class c = 7, luminosity class g = 8, luminosity class d --- BCS3 HR/BS number The HR/BS number is provided if identified in the Yale Catalog of Bright Stars, Third edition (1964). --- GC GC number The GC number is provided if identified in the Boss General Catalog of 33342 Stars for the Epoch 1950 (1937). --- SAO DM number The DM number is provided if identified in the Smithsonian Astrophysical Observatory (SAO) Star Catalog (1966). --- GCVS Star name The star name is provided if identified in the General Catalog of Variable Stars, Volumes 1 and 2 (1958). --- RAs_SAO RA difference (seconds) These are the position differences, infrared catalog-SAO Star Catalog or, if no SAO identification is avalable, the position difference, infrared catalog-variable star catalog. Note: The data file ordered by increasing right ascension (rasort.dat) is also available. Declination Zones (degrees) Sequential Record Number -33 to -25 1-472 -25 to -15 473-1116 -15 to - 5 1117-1725 - 5 to + 5 1726-2262 + 5 to +15 2263-2807 +15 to +25 2808-3365 +25 to +35 3366-3887 +35 to +45 3888-4435 +45 to +55 4436-4919 +55 to +65 4920-5353 +65 to +75 5354-5555 +75 to +81 5556-5612 s DEm_dif Declination difference (arc min) arcmin RArad Right ascension 1950 (radians) rad DErad Declination 1950 (radians) rad Chi-square Excess ID Two-Micron Sky Survey number (TMSS) --- o_ID Total number of obs. of this star Up to three observations are listed in one logical record. This number is repeated in each record containing data for this star. --- Kmag K magnitude of star mag std_Kmag Standard deviation of K magnitude mag Imag I magnitude of star Ignore if I magnitude > 14.0. mag std_Imag Standard deviation of I magnitude Ignore if I magnitude > 14.0 or if byte 28 = 1. mag n_Imag I magnitude questionable = 1, if I magnitude is questionable; = 0, otherwise If I magnitude is 1, then the standard deviation given in bytes 24-27 should be ignored. --- JD Julian day no. of obs. minus 2430000 d Kmag2 K magnitude of star If more than one observation is included in this record, the format for bytes 10-32 is repeated as bytes 34-56. mag std_Kmag2 Standard deviation of K magnitude mag Imag2 I magnitude of star Ignore if I magnitude > 14.0. mag std_Imag2 Standard deviation of I magnitude Ignore if I magnitude > 14.0 or if byte 52 = 1. mag n_Imag2 I magnitude questionable = 1, if I magnitude is questionable; = 0, otherwise --- JD2 Julian day no. of obs. minus 2430000 d Kmag3 K magnitude of star If there is a third observation included in this record, the format for bytes 10-32 is repeated as bytes 58-80. mag std_Kmag3 Standard deviation of K magnitude mag Imag3 I magnitude of star Ignore if I magnitude > 14.0. mag std_Imag3 Standard deviation of I magnitude Ignore if I magnitude > 14.0 or if byte 76 = 1. mag n_Imag3 I magnitude questionable = 1, if I magnitude is questionable; = 0, otherwise --- JD3 Julian day no. of obs. minus 2430000 --- Remarks ID Two-Micron Sky Survey number (TMSS) --- n_ID Remarks --- Melissa C. Larkin SSDOO/ADC 1997 May 27 The original ADC documentation (1991) by Theresa A. Nagy was used to create this ReadMe file. She also did the original data reformatting. UNKNOWN UNKNOWN The Two-Micron Sky Survey Catalogue by G. Neugebauer and R. B. Leighton was published in 1969 as a National Aeronautics and Space Administration (NASA) special publication (NASA SP-3047). A computer program was written to perform the following operations on the original version of the catalogue: - Convert all "&" to "+" - Concatenate left- and right-hand pages into a single data record per entry - Delete catalogue number from the right-hand page data - Add a sequential counter for each record - Combine all entries from 12 original files into a single file for data in catalogue - Combine all measurements of chi-square excess stars from the 12 original files into a single sequential file - Compute and include right ascension and declination in radians at the end of each record in data file - Combine all remarks from the 12 original files into a single sequential file - Reblock main catalogue from 84 bytes to 17000 - Change logical record length from 84 to 170 to accommodate re-organization II_2B.xml UBV Photometry of Bright Stars 2005 II/5 UBV Photometry of Bright Stars UBV Photometry of Bright Stars H L Johnson R I Mitchell B Iriarte W Z Wisniewski Commun. Lunar & Planet. Lab. 4 99, Table 9 ??? ??? 1966 1966CoLPL...4...99J Photometry, UBV Stars, bright The data presented in this catalogue are the results of multicolor photo- metric observations of stars listed in the Bright Star Catalog. Observations were made on the 21-in, 28-in and 60-in telescopes of the Lunar and Planetary Laboratory, and at Tonanzintla Observatory on the 40-in telescope of the Observatorio Astronomico Nacional, Universidad Nacional de Mexico. This catalog of UBV photometry on almost 5000 bright stars covers the entire sky by including southern Cape photometry trans- formed to the UBV system.
Data code Coded number see the file numsys.dat (J.Cl. Mermilliod, CDS, RISP 5) --- rem Remark D = double star V = variable star N = non member of any cluster 1 = A component of multiple 2 = B component of multiple --- V V magnitude mag B-V (B-V) Color index mag U-B (U-B) Color index mag n_N Remark on N * = the number or measurements is at least the one indicated / = the number of measurements has not been published blank otherwise --- N Number of measurements ('STD' for standard) --- Definition of the coded numbering system text Definition of the coded numbering system --- Julie Anne Watko SSDOO/ADC 1996 Aug 15 II_5.xml UBVRIJKLMNH Photoelectric Photometric Catalogue 2007A II/7A UBVRIJKLMNH Photoelectric Photometric Cat UBVRIJKLMNH Photoelectric Photometric Catalogue M Morel P Magnenat Astron. Astrophys. Suppl. 34 477 1978 1978A&AS...34..477M II/116 : ADC CD-ROM vol. 1 \PHOTOM\11COLOR Johnson H.L. 1965, Astrophys. J., 141, 923 Johnson H.L., McArthur J.W., and Mitchell R.J. 1968, Astrophys. J., 152, 465 Mermilliod J.Cl. 1978, CDS Inform. Bull., 14, pp. 32-61 Morel M. and Magnenat P. 1978, Astron. Astrophys. Suppl., 34, 477 Photometry, UBVRIJKLMNH The catalog contains the results from star brightness measures in the first ten (UBVRIJKLMN) broad wavelength bands (Johnson 1965) and the additional bandpass H (Johnson et al. 1968). Data in the above system that have been published up to June 1977 are included. The source reference (Morel and Magnenat 1978) states that there are 5943 entries in the data set with data for 4494 stars. However, a count of the records by coded number shows that there are only 4486 unique entries (not 4494). The catalog includes coded identification numbers (Geneva system), 11 magnitudes, numbers of measurements in each filter, and references.
Catalog Data LID Coded identification number (Lausanne/Geneva identifier) The data on the magnetic tape is ordered by the coded numbers (cf. Mermilliod J. Cl. 1978, CDS Information Bulletin, 14, 32). This numbering scheme has the form +/- C.XXXXXXXX where C has values 0 to 9 inclusive. For reference the following statistics were determined for this catalogue: C #Entries #Unique Entries Short Description 0 340 268 DM catalogues 1 3479 2476 HD and HDE 2 630 564 NGC clusters 3 43 34 IC clusters 4 38 38 Anonymous clusters (< 100) 5 563 407 Anonymous clusters ( >100) 6 394 338 Catalogues and lists of stars 7 0 0 Selected area stars 8 72 61 Catalogues ordered by declination zones 9 384 300 Stellar associations and nearby galaxies Totals 5943 4486 --- n_LID Suffix to LID Symbol Entries Significance D 231 Unresolved binary 1 21 Component A of a double star 2 19 Component B of a double star 3 4 Component C of a multiple star system S 0 Supplementary star in a list, possessing the same identification as another one, followed by "a" or "s". V 359 Indicates variability % 1 (9.00010596) blank 5308 --- U U magnitude: 0.36, 0.36 Explanations for magnitudes are organized as follows. Magnitude: mean wavelength, effective wavelength in microns mag B B magnitude: 0.44, 0.45 mag V V magnitude: 0.55, 0.555 mag R R magnitude: 0.70, 0.67 mag I I magnitude: 0.88, 0.87 mag J J magnitude: 1.25, 1.20 mag K K magnitude: 2.2, 2.20 mag L L magnitude: 3.5-3.4, 3.50 mag M M magnitude: 5.0, 5.0 mag N N magnitude: 10.4, 9.0 mag H H magnitude: 1.62, 1.62 mag o_U Number of measurements for U filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_B Number of measurements for B filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_V Number of measurements for V filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_R Number of measurements for R filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_I Number of measurements for I filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_J Number of measurements for J filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_K Number of measurements for K filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_L Number of measurements for L filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_M Number of measurements for M filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_N Number of measurements for N filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- o_H Number of measurements for H filter Numbers of measurements in each filter. 9999 number of measurements unknown 8XXX minimum number of measurements = 8XXX-8000 7777 this is a Standard for given bandpass --- rem An eventual remark A remark A,B,C... for some variable stars indicating the order of measurements --- ref Reference number (see file: refs) --- References ref Reference number --- text Reference in standard format author(s), year, publication, volume, page --- Julie Anne Watko SSDOO/ADC 1996 May 01 Documentation for the machine-readable version of the UBVRIJKLMNH Photo- electric Photometric Catalogue was originally written by Theresa A. Nagy and Robert S. Hill in July 1980 at ADC (Contract NAS 5-25369). An Intro file was created at CDS on 22-Jun-1994 This ReadMe document is an adjustment of these previous documents to the current CDS standard 01-MAY-1996. II_7A.xml Catalogue of UVBGRI (Stebbins and Withford) measurements: Published data and Weighted Means 2008 II/8 Catalogue of UVBGRI measurements Catalogue of UVBGRI (Stebbins and Withford) measurements: Published data and Weighted Means C Nicollier Rapport Interne CDS 2, updated ??? ??? 1975 1975 II/75 : R and I magnitudes compiled by Jasniewicz (1982) Jasniewicz B., 1982, A&AS 49, 99 (Catalogue: II/75) Kron G.E., Guetter H.H., Riepe B.Y., 1972, Publ. U.S. Naval Obs. 20, part 5. Stebbins J., Withford A.E., 1943, ApJ 98, 20 =1943ApJ....98...20S Photometry, UVBGRI This compilation contains the published results and the weighted means of the observations in the photoelectric photometric system described by Stebbins and Withford (1943). The six filters were selected to give nearly the same response in each of the six spectral regions for a solar-type star. The mean wavelengths or the filters are: ---------------------------------------------------- Filter U B V G R I Wavelength (nm) 353 422 488 570 719 1030 ---------------------------------------------------- The reduction of this system is made in order that (B+G+R) = 0.
Mean photometric colours Published Measurements LID Identification in Lausanne/Geneve system number=1 Keys to the code are described in file "codes"; 'D' in column m_LID indicates a double star with both components measured simultaneously; '1' and '2' in column m_LID indicates components of a composite system. --- m_LID Multiplicity indicator number=1 Keys to the code are described in file "codes"; 'D' in column m_LID indicates a double star with both components measured simultaneously; '1' and '2' in column m_LID indicates components of a composite system. --- Umag Colour in Ultra filter number=2 See Description above; the colours are such that (B+G+R) = 0. mag Vmag Colour in Violet filter number=2 See Description above; the colours are such that (B+G+R) = 0. mag Bmag Colour in Blue filter number=2 See Description above; the colours are such that (B+G+R) = 0. mag Gmag Colour in Green filter number=2 See Description above; the colours are such that (B+G+R) = 0. mag Rmag Colour in Red filter number=2 See Description above; the colours are such that (B+G+R) = 0. mag Imag Colour in Infra filter number=2 See Description above; the colours are such that (B+G+R) = 0. mag n_Nmes Remark on Nmes number=3 Values only for "obs" file. '/' in column n_Nmes indicates an unknown Nmes value, '*' in column n_Nmes indicates that Nmes represents a minimal value. --- Nmes Number of measurements number=3 Values only for "obs" file. '/' in column n_Nmes indicates an unknown Nmes value, '*' in column n_Nmes indicates that Nmes represents a minimal value. --- Ref Reference (see file refs) number=3 Values only for "obs" file. '/' in column n_Nmes indicates an unknown Nmes value, '*' in column n_Nmes indicates that Nmes represents a minimal value. --- References of observations Ref Reference number --- Kron The parenthesized letter number=4 blank for continuation --- Text Text of reference number=5 indicates a reference in Kron et al. (1972) --- Description of LID identification system text Description of LID identification system --- Francois Ochsenbein CDS revised J.A. Watko SSDOO/ADC 1996 Mar 14 UNKNOWN UNKNOWN * July 1975: Magnetic tape with data provided to CDS by M. Mermilliod (Lausanne/Geneva Observatory) * September 1995: documentation produced at CDS * March 1996: Online documentation standardized at ADC II_8.xml Catalogue of Photometric Measurements in the UBVr 20 System 2015 II/15 Photometric Measurements in the UBVr 20 System Catalogue of Photometric Measurements in the UBVr 20 System P Magnenat CDS Internal Report No. 6 ??? ??? 1973 1973 Photometry, UBVr20 Colors In the UBVr photometric system defined by Sandage and Smith (1963), (U-B)20, (B-V)20, and (V-r)20 color indices are given for stars from ten reference lists, along with a LID coded number, V magnitude, number of observations and reference. A list of weighted means is included for stars appearing on more than one list. The reference list and an explanation of the coded numbering system are included in separate files.
The UBVr system is defined by Sandage and Smith (1963). The then recent availability of photomultipliers with S20 cathodes sensitive to the wavelength range 3000 to 8000 A suggested that the customary tricolor photometric system could be extended to include a red point close to 6700 A. The V-r color index can be employed as a good indicator of effective temperature, thanks to its relatively small blanketing effect, compared to B-V. Sandage and Smith also tried to obtain the U, B and V colors as closely as possible to those of Johnson and Morgan's system. In 1960, 64 standard stars of the UBV system (Johnson and Morgan 1953; Johnson and Harris 1954) were measured. Comparison of colors obtained in the natural photometric system ubvr 20 with colors from Johnson, Morgan and Harris give: B-V = 1.100(b-v)20 + 1.023 +/-0.004 +-/0.003 U-B = 1.015(u-b)20 - 1.575 +/-0.003 +/-0.006 (Sandage and Smith 1963) These equations show that the UBVr 20 system is close to the UBV system without being identical. Means were calculated for stars appearing in multiple references according to the customary manner at CDS, based on the number of measures and the weight of each list. All ten lists were given weight 4.
Observations of UBVr 20 colors Weighted means for stars in multiple lists LID Coded number (see codes.dat) Defined in J.Cl. Mermilliod, CDS RISP 5 (see codes.dat) --- rem Remark D = a multiple system 1 or 2 = only one component of a binary was measured --- U-B20 (U-B)20 index If either field is empty, that signifies that the star was not measured on the filters in question. mag B-V20 (B-V)20 index mag V-r20 (V-r)20 index mag n_N Remark about N (obs.dat only) / = N is unknown (1 is assumed) * = N is a minimum number blank = N is exact --- N Number of measurements (obs.dat only) --- V V magnitude mag ref Reference number (see refs.dat) --- References to individual lists ref Reference number --- text Reference (multiline) --- Definition of the coded numbering system text Definition of the coded numbering system ampersands "&" in data files have been changed to "+" --- Julie Anne Watko SSDOO/ADC 1996 May 30 The text of the introduction is taken from P. Magnenat [CDS], translated from French to English by J.A. Watko [SSDOO/ADC]. II_15.xml Catalogue des Mesures Photometriques dans le Systeme (102, 65, 62) de Eggen: Catalogue of Individual Measures; Catalogue of Averages 2018 II/18 Photometric Measurements, Eggen Catalogue des Mesures Photometriques dans le Systeme (102, 65, 62) de Eggen: Catalogue of Individual Measures; Catalogue of Averages P Magnenat CDS Internal Report No. 7 ??? ??? 1974 1974 Photometry, 102, 65, 62 Photometry, Eggen A catalog of photometric measures in Eggen's (102, 65, 62) system has been compiled at the Institut d'Astronomie de l'Universite de Lausanne. A catalog of individual observations and of weighted means are included, with an explanation of the coded numbering system.
Observations Weighted Means LID LID coded number (see codes.dat) --- rem Remark D = a multiple system --- (102) m(102) magnitude mag (65,62) (65, 62) color index = m(62) - m(65). mag (102,65) (102, 65) index = m(102) - m(65). mag n_N Remark about N (obs.dat only) * = N is a minimum number / = N is unknown (1 is assumed) --- N Number of measurements (obs.dat only) 'STD' = a standard star --- ignore Ignore (obs.dat only) --- ref Bibliographical reference num. (obs.dat only) See References section at the end of this document. --- Definition of the Coded Numbering System text Definition of the coded numbering system Definition of the coded numbering system (from J. Cl. Mermilliod, CDS RISP 5) ampersands "&" have been changed to "+" in data files --- Julie Anne Watko SSDOO/ADC 1996 JUL 15 Julie Anne Watko [ADC] thanks Francois Ochsenbein [CDS] for his help in identifying and correcting format errors in the data. II_18.xml The Spatial Distribution of Young Stars in Vela 2020 II/20 UBV Photometry of O & B Stars in Vela The Spatial Distribution of Young Stars in Vela J Denoyelle Astron. Astrophys. Suppl. Ser. 27 343 1977 1977A&AS...27..343D Reddening Photometry, UBV Colors Stars, OB Photoelectric UBV values, derived from observations made at the Boyden and ESO observatories, are presented for 358 early-type stars in the Vela section of the southern Milky Way.
Data rec Record number (if several records for star) --- Seq Running number --- HD HD number --- CPD Cape Photographic Durch. (or CD) --- n_CPD * = CPDzone,num are from Cordoba Durch. --- RAh Right Ascension (1950) hours h RAm Right Ascension (1950) minutes min DE- Declination (1950) sign --- DEd Declination (1950) degrees deg DEm Declination (1950) arcminutes arcmin GLON Galactic longitude deg GLAT Galactic latitude deg Vmag V magnitude 99.99 indicates that the datum is missing. mag u_Vmag Uncertainty flag for V --- B-V (B-V) color index mag u_B-V Uncertainty flag for B-V --- U-B (U-B) color index mag u_U-B Uncertainty flag for U-B --- Sp MK or HD spectral classification --- ref Number of the source for MK Dp. --- Emission E = Halpha emission noted on red plates --- Sp2 Spectral type obtained from Q method --- Q Q parameter Q = (U-B) - 0.72 (B-V) mag E(B-V) (B-V) colour excess mag A(V) A(V) parameter A(V) = 3 x E(B-V) mag m-M Distance modulus mag R Distance of the star pc Z Distance from the galactic plane Z = R*sin(GLAT) pc Nobs Number of observations --- rem * = Comment exists for this star --- Julie Anne Watko SSDOO/ADC 1996 May 24 II_20.xml Narrow-Band Photometry of Late-Type Stars 2021A II/21A Narrow-Band Photometry of Late-Type Stars Narrow-Band Photometry of Late-Type Stars L Haeggkvist T Oja Astron. Astrophys. Suppl. Ser. 1 199 1970 1970A&AS....1..199H Photometry, narrow-band Stars, late-type The catalog is a compilation of photoelectric photometry obtained as part of a program investigating the distribution of stars and stellar matter perpendicular to the galactic plane. Compared to the publication, the "catalog" file does not include the position, the spectral type, the source of the UBV photometry, and neither the number of measurements in the narrow-band filters. The narrow-band filters are: ----------------------------------------------- m(4508) centered at 450.8nm, half-width=5.0nm m(4269) centered at 426.9nm, half-width=4.3nm m(4176) centered at 417.6nm, half-width=4.0nm ----------------------------------------------- ge = m(4269) - m(4508) measures the break at the G-band ce = m(4176) - m(4269) measures the CN absorption.
The catalogue of photometric data HR/BD Designation in Bright Star Catalogue <V/50> or Bonner Durchmusterung <I/122> --- Vmag Visual magnitude in Johnson system mag B-V Colour in Johnson system mag U-B Colour in Johnson system mag m(4508) Magnitude in narrow-band filter number=1 see above in the Decription the filter definition. mag ge = m(4269) - m(4508) number=1 see above in the Decription the filter definition. mag ce = m(4176) - m(4269) number=1 see above in the Decription the filter definition. mag Rem Remark number=2 remarks are as follows: V=variable; D=double star, magnitude difference less than 4mag R=individual remark as follows: HR 1457 : The individual values of Vmag indicate variability HR 1845 : CE Tau HR 2742 : BZ Cam HR 4057/8: The individual values of Vmag indicate variability HR 5490 : W Boo HR 5505/6: Spectral type A2V+K0II-II HR 5512 : The 3 measurements of m(4508) have an amplitude of 0.4mag HR 5589 : RR UMi HR 6406/7: Spectral type M5II + (G5III?+F2?) HR 7157 : R Lyr HR 7735 : V695 Cyg HR 7956 : T Cyg HR 8383 : VV Cep --- Seq Sequential number --- Joseph Florsch, Francois Ochsenbein CDS 1995 Oct 12 UNKNOWN UNKNOWN * Tape received at CDS before 1976 * 25-Sep-1995: First documentation by Gail L. Schneider [SSDOO/ADC] * 12-Oct-1995: Reformatted the "HR/BD" column at CDS II_21A.xml H-{Alpha} Photometry of Late-Type Stars I. F-, G- and K-Type Stars North of the Equator 2024 II/24 H-{Alpha} Phot Late-Type Stars I. Northern F, G, K Stars H-{Alpha} Photometry of Late-Type Stars I. F-, G- and K-Type Stars North of the Equator D W Peat Mon. Not. R. Astron. Soc. 128 435 1964 1964MNRAS.128..435P Photometry, H-alpha Stars, late-type Stars, dwarfs Observations are presented of the strength of the H-{alpha} absorption line in the spectra of approximately 600 northern F, G and K stars of differing luminosities and chemical compositions. Most of the stars in this catalogue were previously observed by Griffin and Redman (1960), Deeming (1960), and Griffin (1961). Data given in this catalog include HD number, MKK spectral classification, high velocity, (B-V) color index, magnesium b ratio, sodium D line ratio and H-{alpha} ratio.
(Peat, 1964) The integrated light-intensity within a band defined by the wavelength limits 6545-6580A, centered on the wavelength of H-{alpha}, was measured by one photomultiplier. The combined integrated light intensity within the two comparison regions defined respectively by the wavelength limits 6477.5 to 6495.0A and 6630.0 to 6647.5A was measured by a second photomultiplier. The wavelengths were monitored using the bright neon emission at lambda 6402 produced by a neon discharge tube, and were held constant to within +-0.5A. Errors of the order of +- 2A in the wavelength setting, however, were found experimentally to have no effect on the results, and corrections for the Doppler shift due to the stellar radial velocity were therefore unnecessary. The "H-{alpha} ratio" R, was defined by the expression R = [B/B(L)]/[A/A(L)] where B, A represent the photomultiplier output counts for a star, in the side bands and H-{alpha} band respectively, and B(L), A(L) represent the corres- ponding counts for the lamp. One might expect this ratio to be partially determined by features, other than H-{alpha}, situated within the central and comparison regions of the stellar spectrum, but examination of a high reso- lution spectrogram of Arcturus (a K2 giant star typical of the stars on the observing program) taken by Griffin (1962) showed that these other features affected the H-{alpha} ratio by less than 0.3%. This is only of the same order as the estimated observational error in the H-{alpha} ratios, and we shall assume therefore that the H-{alpha} ratio is determined solely by the strength of the H-{alpha} absorption line. Griffin (1961) describes the three-channel spectrophotometer with which observations were made at the coude focus of the Cambridge Observatory 36 in reflecting telescope. Griffin and Redman (1959), Deeming (1960), and Griffin (1961) describe the method of Observation and reduction.
Data HD "HD" --- HDnum HD number of the star --- Sp MKK spectral classification --- lum Luminosity class indication 10: Ia 13: Iab 14: Iab-Ib 15: Ib 17: Ib-II 20: II 25: II-III 30: III 35: III-IV 40: IV 45: IV-V 50: V --- HV High Velocity 'HV' indicates that the star is a high velocity star with a space motion in excess of 63 km/s as determined by Eggen (1962). --- B-V (B-V) color index from Deeming (1960) and Argue (1962) mag Mgb Mg b ratio measured by Deeming (1960) --- NaD Sodium D line ratio measured by Griffin (1961) --- Ha H {alpha} ratio --- ID Star number --- Julie Anne Watko SSDOO/ADC 1996 May 10 II_24.xml Catalogue of early-type stars measured in a narrow-band photometric system 2026A II/26A Narrow-band photometry of Early-type stars Catalogue of early-type stars measured in a narrow-band photometric system N Morguleff M Gerbaldi Astron. Astrophys. Suppl. Ser. 19 189 1975 1975A&AS...19..189M Photometry Stars, early-type A compilation of the photoelectric measurements in the Barbier-Morguleff system is presented for 773 stars of spectral types O8 to F6. 706 stars have been measured at least twice. The passbands (in Angstroems) and the mean photometric errors of the indexes C(j)-C(2) (in magnitudes) are: ----------------------- Band Interval m.e. ----------------------- C(1) 6000-5900 0.0318 C(2) 5000-4900 --- C(3) 4905-4815 0.0073 C(4) 4380-4310 0.0100 C(5) 4070-4010 0.0102 C(6) 3965-3925 0.0201 C(7) 3780-3720 0.0195 C(8) 3650-3575 0.0189 ----------------------- Regarding the catalog Pass Bands Morguleff and Gerbaldi (1975) note the following: These spectral intervals permit the determination of certain physical characteristics .... The pass bands 1 and 5 lead us to calculate red and blue gradients. The equivalent widths of the H(beta), H(gamma) lines of hydrogen and the K lines of Ca II are derived from band 3, 4, and 6. Bands 7 and 8 measure the Balmer jump. Listed in the catalog file are the normalized magnitudes corresponding to the above pass bands. The normalized magnitude of a pass band, C(j), is defined as the color index of the magnitude in the band minus the magnitude of the second band, C(2). See Morguleff and Gerbaldi (1975) for a brief discussion of conservation of the system and mean errors across all stars.
The catalogue Name HD or BD (if starting with a + sign) identification HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. --- Var 'V' indicates a variable star number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. --- c1 Index C(1)-C(2). The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. mag c3 Index C(3)-C(2). number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. mag c4 Index C(4)-C(2). number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. mag c5 Index C(5)-C(2). number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. mag c6 Index C(6)-C(2). number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. mag c7 Index C(7)-C(2). number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. mag c8 Index C(8)-C(2). number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. mag Obs Number of measurements Number of measurements contributing to the above values. number= HD or BD number of the object. Only the last two objects have BD rather than HD numbers. number= The normalized magnitudes in seven of the eight pass bands (see "Pass Bands"). C(2) is always equal to zero, by definition. number= Number of measurements contributing to the above values. --- e_c1 Mean error on c1 number=1 the mean error is only computed if Obs>1 mag e_c3 Mean error on c3 number=1 the mean error is only computed if Obs>1 mag e_c4 Mean error on c4 number=1 the mean error is only computed if Obs>1 mag e_c5 Mean error on c5 number=1 the mean error is only computed if Obs>1 mag e_c6 Mean error on c6 number=1 the mean error is only computed if Obs>1 mag e_c7 Mean error on c7 number=1 the mean error is only computed if Obs>1 mag e_c8 Mean error on c8 number=1 the mean error is only computed if Obs>1 mag Francois Ochsenbein CDS and N. Paul Kuin ADC/SSDOO/NASA 1995 Mar 29 UNKNOWN UNKNOWN * Catalogue received at CDS in 1975 (punched cards) * January 1995: standardised description, added 'V' symbol for variable stars listed in the paper. * March 1995: included pertinent information from original ADC documentation to the catalog by N. Paul Kuin. II_26A.xml Catalogue of Photoelectric Photometric Measurements in the UcBV System 2027 II/27 Photoelectric Photometric Measurements, UcBV System Catalogue of Photoelectric Photometric Measurements in the UcBV System B Nicolet A&AS 22 239 1975 1975A&AS...22..239N Photometry, UcBV Colors All measurements in the literature on the Cape photometric system as of early 1975 have been compiled. The catalog includes measurements from 38 publications as well as 469 unpublished measurements forwarded by Dr. A. W. J. Cousins.
The method and computer program described by Hauck (1973) and used by Lindemann and Hauck (1973) was used for the ubvybeta system. The data of Cousins and Stoy (1963) were used as the standard but no systematic differences were found. As the standard error was sufficiently small, each publication was given the same weight. However, Johnson et al (1966) have signaled a slight divergence between their measurements in V and B-V and those given in the Cape system. Account was taken of this in the calculation. The probable error in each magnitude and color is less than 0.01 mag.
Observations NC Coded Number see nmsys.dat --- rem Remark D if the star is a multiple system V if it is a (slightly) variable star --- V V Magnitude mag B-V B-V Color Index index from Cape photometric system mag U-Bc U-Bc Color Index index from Cape photometric system mag n Number of Observations Number of Observations in the following format: " nn" exactly nn observations "* nn" at least nn observations " / " unknown number (1 is assumed for the weighted mean) " STD" the star is a standard star for a publication --- ref Reference Number Reference number: "02nnn" where "02" means UcBV photometric system and "nnn" is the running number in the reference file (file3, part 1) --- Weighted Means NC Coded Number see nmsys.dat --- Rem Remark D if the star is a multiple system V if it is a (slightly) variable star --- V V magnitude mag B-V B-V Color Index index from Cape photometric system --- U-Bc U-Bc Color Index index from Cape photometric system --- References num Reference number --- ref References Number and Reference of the papers used in obs.dat --- Numbering System num Numbering system Description of the coded numbering system used in obs.dat and wtdmns.dat Mermilliod J.Cl., CDS, RISP 5 --- Cross Index NC Coded Number for stars in clusters see nmsys.dat --- HD HD number --- DM Durchmusterung identification --- Julie Anne Watko SSDOO/ADC 1996 Feb 21 II_27.xml Four-colour uvby photometry for bright O to G0 type stars south of declination +10 degrees 2033 II/33 uvby-beta Photometry for Bright O-G0 Southern Stars Four-colour uvby photometry for bright O to G0 type stars south of declination +10 degrees B Gronbech E H Olsen Astron. Astrophys. Suppl. Ser. 25 213 1976 1976A&AS...25..213G Four-colour uvby photometry for bright O to G0 type stars south of declination +10 degrees B Gronbech E H Olsen Astron. Astrophys. Suppl. Ser. 27 443 1977 1977A&AS...27..443G II/215 : uvby-beta Catalogue (Hauck+ 1997), references 137 (uvby data) and 164 (H-beta data) Gronbech B. and Olsen E.H. (1976) Astron. Astrophys. Suppl. Ser. 25, 213 Gronbech B. and Olsen E.H. (1977) Astron. Astrophys. Suppl. Ser. 27, 443 Photometry, uvby, beta Stars, bright The catalog includes for each star as described in the title, the CDS number, HR number, V magnitude, (b-y) color index, m1, c1, beta, mean errors, sum of remarks. The rms errors of one observation are 0.013 mag, 0.005 mag, 0.006 mag and 0.008 mag for V, (b-y), m1 and c1, respectively.
The catalogue CDS CDS number for uvby beta photometry --- ID HR number HR number (from Yale Catalogue of Bright Stars, see catalog <V/50>) and components letters for multiple system For a few stars HD or CD numbers are given --- Vmag V magnitude of the UBV system The value given is a weighted mean of the single observation. Most nights have been given weight 1, one night, weight 0.2, and the rest, weight 0.5 mag e_Vmag Mean error of one observation of Vmag mag b-y (b-y) color index mag e_b-y Mean error for (b-y) mag m1 m1 - (v-b) - (b-y) mag e_m1 Mean error for m1 mag c1 c1 = (u-v) - (v-b) mag e_c1 Mean error for c1 mag P1 Sum of the weights for uvby photometry For fainter stars, the individual observations have been scrutinized and rather low weights have been assigned according to the number of photons counted, etc. For a few stars the weight is zero but the photometry has nevertheless been given, because at least it tells if the star is of early or late type. --- M1 Number of nights the star was observed --- rem1 An asterisk draws attention to a note --- beta Beta index (Crawford-Mander system): a weighted mean mag e_beta Mean error for beta mag P2 Sum of the weights for HBeta photometry --- M2 Number of nights the star was observed --- rem2 An asterisk draws attention to a note --- Julie Anne Watko SSDOO/ADC 1996 Apr 09 UNKNOWN UNKNOWN uvby photometry data were in catalog II/30 . II_33.xml Polarization Catalog 2034A II/34A Polarization Catalogue Polarization Catalog D S Mathewson V I Ford G Klare Th Neckel J Krautter Bull. Inform. CDS 14 115 1978 1978BICDS..14..115M II/178 : "A Catalogue of Linear Polarization Measurements" by Axon and Ellis (1976MNRAS.177..499A) Polarization The catalogue is an extension of the catalogue compiled by Mathewson and Ford (1970MmRAS..74..139M) and the list by Klare and Neckel (1977A&AS...27..215K).
The catalogue of Polarization data Name Identification of the star number=1 names starting by + or - are DM (BD, CD, CPD) designations; names starting by a digit are HD numbers. --- GLON Galactic longitude deg GLAT Galactic latitude deg pol Degree of polarization % galPA Position angle of the E vector in galactic coordinates deg n_galPA Correction performed number=5 2 stars were corrected in December 1997, marked by an asterisk in this position (see Historical Notes) --- eqPA Position angle of the E vector in equatorial coordinates deg RAh Right Ascension 1950 (hours) number=2 this field was computed from GLON and GLAT for stars from Reference 6 (see Historical Notes) h RAm Right Ascension 1950 (minutes) number=2 this field was computed from GLON and GLAT for stars from Reference 6 (see Historical Notes) min DE- Declination 1950 (sign) number=2 this field was computed from GLON and GLAT for stars from Reference 6 (see Historical Notes) --- DEd Declination 1950 (degrees) number=2 this field was computed from GLON and GLAT for stars from Reference 6 (see Historical Notes) deg DEm Declination 1950 (minutes) number=2 this field was computed from GLON and GLAT for stars from Reference 6 (see Historical Notes) arcmin Vmag Visual magnitude mag SpType Spectral type number=3 "II-" stands for "II-III", and "-IV" stands for "III-IV" --- Av Visual absorption mag n_Av '*' when no photometry was available --- m-M Distance modulus (= 5.log(r/10)) mag Ref Reference of the data number=4 References are 0: unidentified 1: Appenzeller I., Zeitschr. Astrophysik =1966ZA.....64..269A 2: Appenzeller I., Astrophys. J. =1968ApJ...151..907A 3: Behr A., 1959, Veroeff. Univ. Sternw. Goettingen N.126 4: Hall J.S., 1958, Publ. U.S. Naval Obs. 2nd Ser. 17, VI 5: van Smith E.P., Astrophys. J. =1956ApJ...124...43V 6: Schmidt T., Zeitschr. Astrophysik =1968ZA.....68..380S 7: Hiltner W.A., Astrophys. J. Suppl. =1956ApJS....2..389H 8: Klare G., Neckel T, =1977A&AS...27..215K 9: Mathewson D.S., Ford V.I., Mem. R. Astron. Soc. 74, 139 =1970MmRAS..74..139M --- Francois Ochsenbein CDS 1997 Dec 17 UNKNOWN UNKNOWN * The tape was received at CDS in 1977 from the authors * February 1996: the catalogue was reformatted in the following way: => the Name of the stars have been changed from 8 to 10 bytes, inserting blanks between zone and numbers of DM designations; => the galactic longitude and latitude, originally in degrees and arc minutes, have been converted into decimal degrees ; => the missing equatorial positions (from Ref. 6) have been computed from the galactic position. * December 1997: errors communicated by Thomas Szeifert, T.Szeifert@lsw.uni-heidelberg.de: the two stars -33 12242 and -29 13809 had a wrong position in the catalogue; the GLON, GLAT, and galPA values were corrected accordingly, and these two stars were set the n_galPA and moved to match the GLON ordering. II_34A.xml Catalogue of Individual UBV and uvbyb Observations in the Region of the Orion OB 1 Association. 2036 II/36 UBV and uvbyb observations of Orion OB1 Association Catalogue of Individual UBV and uvbyb Observations in the Region of the Orion OB 1 Association. W H Warren Jr. J E Hesser Astrophys. J. Suppl. 34 115 1977 1977ApJS...34..115W Photometry, UBV Photometry, uvby, beta Stars, OB The Catalogue of Individual UBV and uvbyb Observations of Stars in the Region of the Orion OB 1 Association presents individual UBV observations of 106 stars in the vicinity of the Orion Nebula (the Sword region) and individual uvbyb observations of 508 stars in all regions of the Orion OB 1 association. For the UBV data the stars are identified by their Brun (1935) numbers, with cross identifications to the chart numbers used in Warren and Hesser (1977); the uvbyb stars are identified by the aforementioned chart numbers and HD, BD or P (=!) (Parenago 1954) numbers in that order of preference. The catalogue contains the data of all observations and is intended to provide data for investigations of variability in the Orion region.
UBV data BRUN Number in the catalogue of Brun (1935) --- WH Number assigned by Warren and Hesser (1977) --- V observed visual magnitude Byte 15 is used only when a night's observations averaged to yield a 5 in the thousandths column. mag n_V : = certain nightly V are discordant The following stars each have a single discordant value which careful inspection of the original data fails to explain; while the existence of these discrepancies may be indicative of variability, it is more likely that they simply reflect an undetected error at the telescope; therefore, they should not be used in forming means; Brun 37 (12.0568) Brun 62 (12.0668) Brun 202 (12.0468) and Brun 244 (12.0468). Star Brun 490 appears variable in V, which Walker's (1969) data weakly suggest too. --- B-V observed B-V Byte 23 is used only when a night's observations averaged to yield a 5 in the thousandths column. mag n_B-V : = uncertain nightly B-V --- U-B observed U-B color Byte 31 is used only when a night's observations averaged to yield a 5 in the thousandths column. mag u_U-B : = uncertain nightly U-B; --- u2_U-B Additional colon if nightly U-B mean very uncertain. --- DATE-OBS Date of observation in form MM.DDYR (12.0468 = 4 December 1968). --- uvby-beta data WH Number assigned by Warren and Hesser (1977) for purposes of chart identification. --- WHCOMP Component in multiple systems --- CAT Catalogue identification The catalog identification HD - Henry Draper Catalogue BD - Bonner Durchmusterung P - Parenago [1954]) --- CAT_NUM Catalogue number (right justified). For BD stars, the first two digits are the zone; the remaining numbers are the number, with zero fill between the numbers and the zone. --- V V magnitude transformed from y. mag b-y b-y color index mag m(1) m(1) color index mag C(1) C(1) color index mag date_uvby UT date of uvby observation in the units indicated (month. dayyear as mm.ddyr). --- b-index b index mag date_b UT date of b observation (mm.ddyr) --- M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1995 Mar 30 UNKNOWN UNKNOWN Record 859 in file ubvybeta.dat has an erroneous value for the V magnitude that needs to be resolved. II_36.xml Catalogue of UBV HR Diagrams of Globular Clusters 2037 II/37 UBV HR Diagrams of Globular Clusters Catalogue of UBV HR Diagrams of Globular Clusters A G D Philip M F Cullen R E White Dudley Obs. Report No. 11 ??? ??? 1976 1976ucmd.proc.....P Clusters, globular HR diagrams UBV observations of over 37,000 stars have been compiled from the literature to yield 165 color-magnitude diagrams. There is a list of bibliographic references for each cluster diagram.
This catalog contains 165 sets of data collected from the literature as of 1976. For many clusters, more than one data set is included. Most of the data is in the form of V and B-V; for some sets, U-B is also given. A few sets are in other systems but have been transformed to UBV. The original publication contains plots of the data so that the color magnitude diagrams can be easily compared. Only the data are given in this version. Stars marked as non-members by the original authors including standard stars, were not included. Also excluded were data which the original authors collected from earlier references. The reference publication also contains extensive tables of data on each cluster. This information can be obtained from other sources, such as the Third Revised Galaxy Catalog. The color excess, E(B-V) is from Burstein and McDonald (1975). If the value is enclosed in parentheses there was no value for E(B-V) in Burstein and McDonald and the value used was taken from Kukarkin (1975). The metal abundance [Fe/H] are from Kukarkin (1974). The spectral type is from Kinman (1959). If the spectral type is enclosed in parentheses the spectral type is taken from Kukarkin (1974). In the reference to the original table of data the first two numbers indicate the date, the rest of the reference follows. In a few cases the catalogue diagram did not check out with the published data. Every star listed in the published catalogue was plotted unless it was individually marked as a non member. A Xerox copy of the original C-M diagram was reproduced in the publication when the source of the difference between the original and the diagram in the catalogue could not be located.
The data ID Identification The ID is normally the NGC number. One data set for omega Centauri is labeled W Cen and some other sets use the cluster name rather than the NGC number. Pal 4 is labeled as such. --- V V Magnitude mag B-V B-V Color Index Seven of the datasets were not originally on the UBV system. The catalog data have been transformed to UBV values. The transformation equations used to transfer these to the UBV system and the references to these equations are as follows: ----------------------------------------------------------------------------- Original Transformation Cluster System Equation Used Reference ----------------------------------------------------------------------------- NGC 5466 P-V B-V=0.92*(P-V) +0.16 (1961, A.J., 66, 71) NGC 6205 C.I. B-V=0.84* C.I, +0.23 (1962, Ap.J., 135, 311) NGC 6254 C. I B-V=0.84* C.I. +0 23 (1962, Ap. J ., 135, 11) NGC 6656 C.I. B-V=0.84* C.I. +0.23 (1959, A.J., 64, 28) NGC 6779 Mpg-V B-V=0.85*(Mpg-V)+0.25 (1965, Asiago Contr, 175,63) NGC 7078 C.I. B-V=0.84* C.I. +0.23 (1962, Ap.J., 135, 311) NGC 7089 C.I. B-V=0.84* C.I. +0.23 (1962, Ap.J., 135, 311) mag U-B U-B Color Index mag n_no1 Remark on Number of Observations? The meaning of this remark is unclear. --- no1 Number of Observations --- no2 Observation type 0 unknown 1 photoelectric 2 photographic --- code Code --- yr Year of publication a ref Reference Journal Volume Page --- Detailed references to the published data name Name Usually NGC number. If blank, then references are continued on next line. --- alt_name Alternate Name --- ref Reference --- The headers name Cluster name --- alt_name Alternate name --- set_no Data set number The data sets are numbered in the order they occur in measures.dat. --- n_E(B-V) Remark on E(B-V) If the value is enclosed in parentheses there was no value for E(B-V) in Burstein and McDonald (1975) and the value used was taken from Kukarkin (1974). --- E(B-V) Color excess in B-V mag paren Parentheses --- Fe/H Abundance index [Fe/H] --- Sp Spectral Type --- yr Year of ref a com Comma --- ref Reference --- Nancy G. Roman SSDOO/ADC Nov-17-1995 J.A. Watko SSDOO/ADC 1995 Dec 18 II_37.xml Photoelectric Measures of Hydrogen-Line Absorption in Early-Type Stars 2040 II/40 Hydrogen-Line Absorption in Early-Type Stars Photoelectric Measures of Hydrogen-Line Absorption in Early-Type Stars M K V Bappu S Chandra N B Sanwal S D Sinvhal Mon. Not. R. Astron. Soc. 123 521 1962 1962MNRAS.123..521B Photometry, hydrogen-line Stars, early-type Photoelectric determinations of H-{gamma} absorption line intensity have been made of stars in selected clusters and associations as well as in the general galactic field. Interference filters having a width at half intensity of 45 A were used to isolate spectral regions centered on 4280 A, H-{gamma} and 4410 A. The {Gamma} indices derived, which represent a measure of H-{gamma} absorption, can be used in conjunction with unreddened values of either (U-B) or (B-V) for spectral and luminosity class determinations of stars in the spectral range O6 to A0.
Data HD Henry Draper number --- V0 V0 magnitude mag (U-B)0 (U_B)0 color index mag Gamma Gamma index {Gamma} * 10^-3 = -2.5 * log[(L*S)^(1/2)/{gamma}] where L, S and {gamma} indicate the respective deflections through the filters that isolate respectively the continuum on the long and short sides and the radiation at the position of the H{gamma} line. --- ID Running number --- Julie Anne Watko SSDOO/ADC 1996 DEC 19 II_40.xml Photoelectric Measurements of the 4200-A CN Band and the G Band in G8-K5 Spectra 2041 II/41 4200-A CN Band and G Band in G8-K5 Spectra Photoelectric Measurements of the 4200-A CN Band and the G Band in G8-K5 Spectra R E Griffin R O Redman Mon. Not. R. Astron. Soc. 120 287 1960 1960MNRAS.120..287G Photometry, CN band Photometry, G band Stars, late-type Measurements of the {lambda} 4200 A CN band are presented for 712 late-type stars. G band data are also included for 212 of these stars. Mean errors of absolute magnitudes derived from CN intensities are at least 1.5 mag. Spectral type determined by G band intensity has a mean deviation of 0.15 class from the MK type for G to K1 stars. The file photom.dat contains 712 data records in the form of CN ratios and G-band ratios, with annotations. The CN ratio is the ratio of the sum of the intensities in the 4097-4149 A and 4230-4283 A wavelength ranges to the intensity in the 4164-4214 A range. The latter contains the CN absorption band, and the first two ranges serve as nearby continuum references. The ratio is a measure of the depth of the absorption in the CN band. Values greater than 2 indicate absorption in the band. The G-band ratio is similarly the ratio of the sum of the intensities in the 4230-4270 A and 4342-4380 A wavelength ranges to the intensity in the 4285-4315 A range.
Catalog Data HD Number of star in the Henry Draper Catalog number=1 In three instances, the star observed has no HD number and this column is left blank. The star is identified in the fourth column. --- CNratio CN-band ratio (x100) --- Gratio G-band ratio (x100) --- Notes Notes to the entries number=2 The following table provides the meaning of the characters in these columns. A Dynamical space velocity greater than 80 km/s B "4150" C "Weak-CN" D "Strong-line" E "Weak-line" F B.D +42.939 deg G Composite spectrum, early-type companion H Double, companion star only partly excluded by slit I Star name: 49 Ser B J Star name: 70 Oph B In the cases of all double stars not indicated with 'H', where the angular separation is less than 2 arcsec, the two stars have been measured together, and where the separation is more than 2 arcsec, the brighter component alone has been observed. --- Julie Anne Watko SSDOO/ADC Seth W. Digel SSDOO 1997 Aug 25 II_41.xml K-Line Photometry of Southern A Stars, Table I: Summary of Data on Southern A Stars 2043 II/43 K-Line Photometry of Southern A Stars, Table I K-Line Photometry of Southern A Stars, Table I: Summary of Data on Southern A Stars R C Henry J E Hesser Astrophys. J. Suppl. 23 421 1971 1971ApJS...23..421H Photometry, K-line Stars, A-type The photoelectric measurements of the strength of the calcium K-line has been extended by 223 stars of predominantly southern or equatorial declinations which are well distributed in right ascension. This has expanded the existent list to 369 field stars for which a k-index is available, including many more Am stars. All available k-index data for field stars are presented here.
The present work represents a continuation of that described previously (Henry 1968, 1969 [hereinafter referenced as Paper I]), in which the K-line of calcium at 3933 A is measured photoelectrically in A-type stars with a narrow-band spectrometer. The result for each star is a K-line-strength index, called k, the value of which appears to depend predominantly only on the temperature of the star and the abundance of calcium in its atmosphere. The temperature dependence is well known; the abundance dependence appears as a correlation between the residual dk in k (after allowance for the temperature effect) and the difference from normal of the general metallicity index [m1] of Stromgren (1966). Alternatively, it was shown in Paper I that the calcium abundance is probably the effective factor in producing the scatter in the relation between k and b-y by a process of elimination of other parameters (luminosity, etc.) that were found not to affect appreciably the value of k. The value of k is, however, affected by a third parameter, namely, whether the star is an Am star or not. Many of the stars of Paper I were reobserved in order to tie in the new measurements with the old ones. An emphasis was laid on observing more Am stars, and on observing some stars that are of somewhat earlier spectral types than the earliest ones observed previously. Simultaneously with the field-star measurements described here, extensive data were acquired for the A stars in five open clusters (Hyades, Pleiades, IC 2391, IC 2602, and NGC 6475) and one association (Orion), as described in Paper III (Hesser and Henry 1971). The observations were made with the same instrument that was used to obtain the data for Paper I, and a description of the instrument may be found in that paper.
Data HR HR Number --- mag Visual Magnitude from BSC. Hoffleit (1964), but, where necessary, from Blanco et al. (1968) mag B-V (B-V)-Color from BSC. mag new New k-Index in Magnitude mag e_new RMS-Error of New k-Index RMS error was not calculated if fewer than 4 observations were available. mag k Final Value of k-Index If fewer than 4 new observations were available, then present data were combined with data from paper I. mag e_k RMS-Error of final k-Index mag dk Deviation of k-Index Deviation of k-index from the normal value for stars of the same color. A positive dk has the sense of an over-abundance of calcium. mag class Class of the Star on the system of Stromgren (1966) L = Late group star (later than A3) I = Intermediate star (A0-A3) E = Early star (B stars) --- b-y (b-y)-Color from Stromgren-Perry Catalogue Stromgren & Perry (1965) and Crawford et al. (1970) mag E(b-y) Color excess Determined by the method of Stromgren. This value has been added to observed (b-y) to obtain the b-y values given in this catalog. mag beta beta-Index Crawford & Mander (1966) and Crawford et al. (1966,1970) mag m1 m1-Reddening-Independent-Index Stromgren (1966) mag dm1 Deviation of m1-Index Deviation of m1-index from the value for normal main-sequence stars. A negative value indicates high metal abundances. mag c1 c1-Reddening-Independent-Index Stromgren (1966) mag dV Magnitudes Above the Main-Sequence The number of magnitudes the star has evolved above the main-sequence calculated from data of c1-index. mag u-b (u-b)-Index of Stromgren mag a a-Index or dm1 For E-group stars this is d(m1) calculated by the alternate method while for i-group stars it is the a-index temperature parameter of Stromgren. mag r r-Luminosity-Index of Stromgren; I-Stars mag ID record number --- Julie Anne Watko SSDOO/ADC 1996 Apr 10 II_43.xml A Reference List for the UBV System 2048 II/48 A Reference List for the UBV System A Reference List for the UBV System B Nicolet Bull. Inf. CDS No. 11, p. 20 ??? ??? 1976 1976BICDS..11...20N II/168 : Catalogue of Homogeneous Means in the UBV System (Mermilliod 1991) Hauck B. 1973, in Ch. Fehrenbach and B.E. Westerlund (eds), Spectral Classification and Multicolour Photometry, p. 285, D. Reidel, Dordrecht Johnson H.L., Mitchell R.I., Iriarte B. and Wisniewski W.Z. 1966, Comm. Lunar and Planet. Lab. no. 63 Lindemann E. and Hauck B. 1973, Astron. Astrophys. Suppl. 11, 119 Mermilliod J.C. 1973, Rapport interne du CDS 5/1973. Mermilliod J.C. and Nicolet B. 1976, in preparation. Nicolet B. 1976, Bull. Inf. CDS No. 11, 20. Photometry, UBV References This catalog is a file of 13422 records giving for each star, an identification, V, B-V, and U-B. Care was taken to place all measurements on the Johnson UBV system by determining possible systematic differences between measurements by Johnson and those by other observers.
The list of Johnson et al. (1966) of 4777 stars was considered as fundamental and given absolute priority. The differences between these data and those for the same stars in other lists in which Johnson was a coauthor were used to determine the systematic corrections and the dispersions were used to determine the weight for each of these lists. Finally, other lists were treated in the same way with absolute priority given to those data in the lists with Johnson as a coauthor.
The catalogue ID Star identification in Geneva system see nmsys.txt (Mermilliod, 1973) --- m_ID ID multiplicity suffix --- Vmag V magnitude mag B-V B-V Color Index mag U-B U-B Color Index mag nmsys.txt Mermilliod numbering system refs.txt References used in 3 step file preparation (table 1 of paper) Julie Anne Watko SSDOO/ADC 1996 May 10 II_48.xml The Catalogue of 10-micron celestial objects 2053 II/53 Catalogue of 10-micron Celestial Objects The Catalogue of 10-micron celestial objects R T Hall Report for Space & Missile System Organisation: SAMSO-TR-74 212 ??? ??? 1974 1974N75-14662.....H Infrared sources Photometry, infrared The published report was prepared by R. T. Hall (1974) for the Space and Missile systems Organization, Air Force System Command. The machine version includes a 10-micrometer catalog number, object name, right ascension and declination (B1950), galactic coordinates (B1950), proper motions, spectral types, magnitudes in the V (0.55 micrometers), I (0.84 mu), K (2.2 mu) and N (10 mu) bands, flux measurements at 10 mu, and cross identifications to the numbering systems of the Durchmusterung catalogs, the SAO catalog, the Bright Star Catalogue, The Henry Draper Catalogue and the GC, and CalTech Two-Micron Sky Survey (Neugebauer and Leighton, 1969) where such identifications exist.
Catalog data CAT 10 micron Catalog Number (left justified) --- Name Star Name Star name hierarchy (1) Bayer Greek alphabetic notation (2) Argelander variable star notation (3) Flamsteed number (4) Bayer Roman alphabetic notation (used as little as possible because of lowercase letters) (5) Other notation Greek letters mu and nu are spelled muu and nuu to eliminate confusion with Argelander variable star notation. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec GLAT Galactic latitude (degrees) deg GLON Galactic longitude (degrees) deg pmRA Right ascension proper motion mu(s,alpha)x1e-4 0.1marcsec pmDE Declination proper motion mu(",delta)x1e-3 marcsec Sp Spectral type, nebula type, or other designation --- sign1 "<", "V", or "b" --- Flux 10 micron Flux/micron (xlO-16W/cm-2/micron). 10-6W/m3 sign2 "V" --- V magnitude in the V band mag I magnitude in the I band mag K magnitude in the K band mag sign3 ">", or "b" --- N magnitude in the N band mag Zonesign Sign of DM number --- Zone Zone of DM number mag DM DM number --- SAO SAO number --- YBS YBS number --- HD HD number --- GC GC number --- CIC CalTech Infrared Catalogue number --- flag1 The value of one in this byte means not last entry; more values will follow in bytes 226-275 A blank means last set of bytes with flux measurements in bytes 153-202. --- Flux_m1* Flux measurements --- Ref1 References (separated by commas) --- flag2 The value of one in this byte means not last entry; more values will follow in bytes 299-314. A blank means last set of bytes with flux measurements in bytes 226-275. --- Flux_m2 Flux measurements separated by commas. --- Ref2 References (separated by commas) --- flag3 There is only one entry with flux measurements in bytes 299-314 and that is 10 micron #050071 (ALPHA ORIO). All of the other entries are blank in bytes 299-321. --- Flux_m3 Flux measurements separated by commas. --- Ref3 References (separated by commas) --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Apr 05 UNKNOWN UNKNOWN The catalogue of 10 micron Celestial Objects was a published report by R. T. Hall (Aerospace Corporation) for the Space and Missile System Organization (report number SAMSO-TR-74-212) in 1974. The catalogue was received in card deck form from Hall through the National Space Science Data Center (NSSDC) at NASA/GSFC. The catalogue was transferred to magnetic tape with an equal number of bytes for each record and changing some special symbols as described below. UNKNOWN UNKNOWN This document includes the original ADC documentation of this catalog prepared by Theresa A. Nagy. Several special characters which are not part of the IBM 360 print chain were changed to correspond with the print chain available on the IBM 360 series at NASA/GSFC. Punch Code Punch Code Symbol Original Card Tape Version Tape Version 12-0 12-4-8 < 12-4-8 12-4-8 < 0-8-2 0-8-6 > 12 12-6-8 + Quantities in the flux/micron (x10-16) field which have any of the symbols (<, <=) should have in the N magnitude field the corresponding opposite relation (>, >=), respectively. In the hard copy of the catalogue there were several pairs which did not have such a one-to-one correspondence, and the following changes were made to correct this situation, assuming in all cases that the relationship associated with the flux/micron value was the "correct" relationship. Ten-Micron N N Catalogue Number Printed Catalogue Tape Version 060011 3.17 >3.17 101081 3.49 >3.49 010301 7.30 >7.30 All of the entries preceded by the symbol "<" in the tape version of the catalogue include those which should be preceded by either the "<" symbol or the "<=" symbol. Since the latter symbol is not available in the print chain on the computer used here at NASA/GSFC, the symbol "<" includes both cases. The following is a list of the ten-micron sources where the value of flux/micron should be preceded by a "<=" sign. 000411 020616 090201 120161 131471 190272 000412 020941 090692 120181 170051 191011 000481 021201 100204 120281 170061 210911 000482 030301 100551 120291 170071 220341 001111 031101 100601 120301 170601 221111 010151 060224 100971 120472 170921 230231 010301 070611 120111 121011 171411 230541 010321 080331 120122 130231 180981 010322 081341 120123 130421 181132 Similarly, all of the above entries should include the equality with the ">" symbol in the N magnitude field. The catalog was reformatted in April 1995 where the implicit decimal point was made explicit. Special symbols were separated from the data values and excessive blank columns were removed. II_53.xml Gershberg Flare Star Catalogue 2055 II/55 Gershberg Flare Star Catalogue Gershberg Flare Star Catalogue N I Shakhovskaya Veroeff. Bamberg IX, 138 ??? ??? 1971 1971 Stars, flare This catalog groups the flare stars as presented in the IAU Colloquium 15 (combined Colloquium of Commisions 27 and 42) held at Bamberg 31-Aug to 03-Sep 1971 entitled "New Directions and New Frontiers in Variable Star Research" The following definition of the UV Cet-type variables was given in Kukarkin's General Catalogue of Variable Stars (1969): "dMe stars, sometimes subject to flares with the amplitude from 1 to 6mag. Maximum brightness is attained in seconds or dozens of seconds after the commencement of the flare; the star returns to its normal brightness after several minutes, or dozens of minutes. A typical representative is UV Ceti." Now it is impossible to consider this definition as a quite right because: 1) There are a number of M-dwarf stars affected by the flares similar to the UV Ceti flares, but in their quiet state spectra, no emission lines are observed. For example, BD+43 44A, BD+43 44 B, and SZ UMa, the flare activity of these stars were detected in Crimea; and probably BD-04 4048B is suspected as a flare star by HERBIG. 2) The lower limit of flare amplitude cited in Kukarkin's corresponds to visual observations, but the modern photoelectric observations register flares with amplitudes to 0.02-0.05mag. Therefore we suppose, that UV Cet-type variables are K-M dwarfs, which show quick flares with amplitudes exceeding the observational errors, and duration of the flares are from a few seconds up to a few hundred minutes. The "catalog" file includes only such variable K-M dwarf stars, for which existing observations allow to construct flare light curves. All stars in "catalog", except V371 Ori, have photoelectric flare light curves. The strong flare of V371 Ori was observed in radio region, but simultaneous optical observations were carried out photographically and visually only.
The catalogue of flare stars Name Designation of the object --- RAdeg Right ascension B1950 (degrees) deg DEdeg Declination B1950 (degrees) deg Rem Remark (Multiplicity, other id., etc.) --- Period Period (for binaries) in days or years depending on x_Period --- x_Period Units in which Period is expressed --- MajAxis Semi-major axis (for binaries) arcsec Remark Other designation (Gliese number) or comment --- Joseph Florsch CDS 1995 Oct 09 UNKNOWN UNKNOWN * The tape was provided by Bamberg Observatory to CDS in 1978 * 09-Oct-1995: catalogue reformatted at CDS II_55.xml The 100-Micron Survey of the Galactic Plane 2056 II/56 100-Micron Survey of the Galactic Plane The 100-Micron Survey of the Galactic Plane W F Hoffmann C L Frederick R J Emery Astrophys. J. 170, L89 ??? ??? 1971 1971ApJ...170L..89H Photometry, infrared Surveys Galactic plane Infrared sources The catalog represents a survey of a portion of the galactic plane at a wavelength of 100 micrometers with a balloon-borne, stabilized, 12-inch infrared telescope having a sensitivity of 10(-22) W/m2/Hz. The survey covers 750 square degrees of the sky, including most of the galactic plane between galactic longitudes of 335 and 88 degrees, plus a number of other selected areas of interest. Seventy-two sources have been detected, 60 of which are identified with continuum radio sources, bright nebulae, dark nebulae, and infrared stars. The catalog includes right ascension and declination (B1950.0), galactic coordinates, 100-micrometer peak flux densities, sizes of sources, and identifications.
Catalog data CAT 100-micron Catalogue Number --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin NGLON New Galactic Longitude (degrees) deg sign Sign of new galactic latitude --- NGLAT New Galactic Latitude (degrees) deg Flux_pk 100um Peak Flux Density unit= 10-22Wm-2Hz-1 10+4Jy Sigma Significance This is the ratio of the correlation of the signal with a function representing the beam profile to the rms noise level of the correlation. --- flag "P" if point source --- size Value of source size in degrees Value of source size is given when the signal-to-noise is sufficient to clearly distinguish the shape of the signal from that of a point source. deg Flux_tot 100um Total Source Flux Density (corrected for source size) unit= 10-22Wm-2Hz-1 10+4Jy Ident Identification R - Radio Continuum I - Radio Combination Lines M - Molecular Lines B - Bright Nebulae D - Dark Nebulae L - Radio Recombination Lines --- rem Remarks --- M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1995 Apr 10 II_56.xml Catalogue of stellar ultraviolet fluxes (TD1): A compilation of absolute stellar fluxes measured by the Sky Survey Telescope (S2/68) aboard the ESRO satellite TD-1 2059B II/59B Catalogue of stellar UV fluxes Catalogue of stellar ultraviolet fluxes (TD1): A compilation of absolute stellar fluxes measured by the Sky Survey Telescope (S2/68) aboard the ESRO satellite TD-1 G I Thompson K Nandy C Jamar A Monfils L Houziaux D J Carnochan R Wilson The Science Research Council, U.K. ??? ??? 1978 1978QB6.C389....... III/39 : UV Bright Star Spectrophotometric Catalog (Jamar et al., 1976) II/86 : Supplement to the UVBS Photometric Catalogue Boksenberg A., Evans R.G., Fowler R.G., Gardner I.S.K., Houziaux L., Humphries C.M., Jamar C., Macau D., Malaise D., Monfils A., Nandy K., Thompson G.I., Wilson R., Wroe H., =1973MNRAS.163..291B Haynes D.S., Latham D.W., =1975ApJ...197..593H Humphries C.M., Jamar C., Malaise D., Wroe H., =1976A&A....49..389H Jamar C., Macau-Hercot D., Monfils A., Thompson G.I., Houziaux L., Wilson R., 1976, "Ultraviolet Bright Star Spectrophotometric Catalogue", ESA Special Report 27 (Cat. <III/39>) Thompson G.I., Nandy K., Jamar C., Monfils A., Houziaux L., Carnochan A., Wilson R., =1979BICDS..17...78T Photometry, ultraviolet (adapted from ADC documentation EAC-T-5294-0028): The Belgian/UK Ultraviolet Sky Survey Telescope (S2/68) in the ESRO TD1 satellite carried out a controlled scan of the whole sky. It measured the absolute ultraviolet flux distribution between 2740A (274nm) and 1350A (135nm) of point sources down to tenth visual magnitude for unreddened early B stars. The S2/68 experiment has been described by Boksenberg et al. (=1973MNRAS.163..291B) and the absolute calibration by Humphries et al. (=1976A&A....49..389H). The catalog contains results from the sky-scan experiment in the TD1 satellite of the European Space Research Organization. The catalog lists the absolute ultraviolet fluxes in four passbands: --------------------------------------------------------- Passband Center: 274.0nm 236.5nm 196.5nm 156.5nm Effective Width: 31.0 33.0 33.0 33.0 --------------------------------------------------------- for 31215 stars. The stars have been selected subject to the constraint that the signal-to-noise ratio should be at least 10.0 in any one of the four passbands. Many of the fainter stars of spectral types later than A5 do not have significant signals in all of the spectrophotometric channels (particularly the 1565A channel). Consequently, after the removal of the background, they can randomly give rise to small negative values of flux. We have decided not to suppress these negative values but to give them together with their error as they can be significant when considered as part of a statistical sample. Although the sky coverage is essentially complete, the catalogue does not contain the fluxes for all stars that fall within the limit of the sensitivity of the instrument. If any star expected to be present is missing, then its signal is probably blended with that of a nearby star in which case the data have been discarded. The fluxes F(lambda), and errors, sigma(lambda), can be transformed to the visual magnitude scale using the absolute calibration of Haynes & Latham (=1975ApJ...197..593H): m(lambda) = -2.5 log10 F(lambda) - 21.175 sigma_m(lambda) = 1.086 sigma(lambda)/F(lambda) Also: F(nu) = 3.336x10^-19^ lambda^2 F(lambda) m(nu) = -2.5 log10 F(lambda) - 5 log10 lambda - 18.724 sigma_m(nu) = 1.086 sigma(lambda)/F(lambda) where F(lambda) is in units of erg.cm^-2^.s^-1^.A^-1^ (mW/m2/(0.1nm)) lambda is in Angstroms and F(nu) is in units of erg.cm^-2^.s^-1^.Hz^-1^ (mW/m2/Hz = 10^23^Jy)
TD 1A
The Catalog of Stellar UV Fluxes TD1 Catalog running number --- HD Henry Draper Catalog number --- UVBSflag '1' if in UVBS Catalog (Jamar et al. 1976) (=III/39A) --- DM Durchmusterung (BD/CD/CPD) designation, as CCsZZNNNNN (catalog, sign, zone number) --- S2/68 S2/68 Catalog Number --- Vmag Visual magnitude mag SpType Spectral type --- RArad Right ascension, 1950.0, in radians rad DErad Declination, 1950.0, in radians rad F2740 =-10.00 Flux in 2740A band (see Exp) 10mW/m2/nm e_F2740 =-1.00 Standard error for F2740 (see Exp) 10mW/m2/nm F2365 =-10.00 Flux in 2365A band (see Exp) 10mW/m2/nm e_F2365 =-1.00 Standard error for F2365 (see Exp) number=1 a few records with standard errors in F2365 and F1965 larger than 100.00 were assigned a value of '99.99'. This occured in records (TD1 numbers): ----------------------------------- TD1 HD Band Error ----------------------------------- 639 6676 1965 133.70 14977 91979 1965 110.22 17270 123445 1965 114.56 18199 137058 2365 119.69 18199 137058 1965 213.83 ----------------------------------- In reference to these specific figures, G. I. Thompson remarks in a private communication: "...the formal computed error has turned out to be so large that the result is probably worthless anyway." 10mW/m2/nm F1965 =-10.00 Flux in 1965A band (see Exp) 10mW/m2/nm e_F1965 =-1.00 Standard error for F1965 (see Exp) number=1 a few records with standard errors in F2365 and F1965 larger than 100.00 were assigned a value of '99.99'. This occured in records (TD1 numbers): ----------------------------------- TD1 HD Band Error ----------------------------------- 639 6676 1965 133.70 14977 91979 1965 110.22 17270 123445 1965 114.56 18199 137058 2365 119.69 18199 137058 1965 213.83 ----------------------------------- In reference to these specific figures, G. I. Thompson remarks in a private communication: "...the formal computed error has turned out to be so large that the result is probably worthless anyway." 10mW/m2/nm F1565 =-10.00 Flux in 1565A band (see Exp) 10mW/m2/nm e_F1565 =-1.00 Standard error for F1565 (see Exp) 10mW/m2/nm Exp 10-base exponent for all Fluxes, e.g. Flux(2740) = 10^Exp^ x F2740 --- Francois Ochsenbein CDS 1995 Oct 24 UNKNOWN UNKNOWN * from ADC Documentation (EAC-T-5294-0028) by Robert S. Hill and Theresa A. Nagy (1981), revised April 1991 by Susan E. Gessner and Lee E. Brotzman, NASA/GSFC: The "Catalogue of Stellar Ultraviolet Fluxes", which represents results from the sky-scan experiment in the TD1 satellite of the European Space Research Organization (ESRO), was received from Dr. G. I. Thompson of the Royal Observatory, Edinburgh, Scotland. The present documentation is mostly a rearrangement of material provided by Dr. Thompson. The tape as received was edited at GSFC as follows: five standard-error values represented by asterisk-filled fields were changed to 99.99. The actual values as given in the hard copy version of the catalogue are given in the "Byte-by-Byte description" above. Some of the pertinent statistics for the data on this tape have been determined. The number of entries which have no valid data for the star as a function of wavelength are: -------------------------- Lamda (A) Entries -------------------------- 2740 5 2365 752 1965 747 1565 735 -------------------------- and, the number of entries that have small negative flux values as a function of wavelength are: -------------------------- Lamda (A) Entries -------------------------- 2740 8 2365 97 1965 154 1565 3392 -------------------------- The catalog was again revised in April 1991. Two byte catalog designations were added to the Durchmusterung numbers. During this process, Dr. Nancy Roman discovered that several of the values given in the original catalogue for the right ascension field (bytes 40-48) were in error. These values were corrected by subtracting 0.0043633 from the original value. The records in which this change occured are: 8703 9546 21996 9322 9671 31105 9509 10112 31139 9414 21723 * October 1991: "Selected Astronomical Catalogs" Vol. 1 CD-ROM, directory /photom/td1 * 24-Oct-1995: Documentation file added at CDS (F. Ochsenbein, J. Florsch) II_59B.xml Catalogue of Extinction data 2062 II/62 Catalogue of Extinction Data Catalogue of Extinction data Th Neckel G Klare M Sarcander Astron. Astrophys. Suppl. Ser. 42 251 1980 1980A&AS...42..251N Catalogue of Extinction data Th Neckel G Klare M Sarcander Bull. Inform. CDS 19 61 1980 1980BICDS..19...61N Extinction interstellar extinction Galaxy: structure Extinction values and distances have been computed from UBV, MK and beta data for more than 11000 O to F stars, including 7565 O and B stars. For 1020 stars two independent distance moduli were derived using MK and beta absolute magnitudes. The mean values of their differences is less than 0.01mag.
The catalogue No Running number --- HD HD number --- HD_m Remarks to HD number number=1 Remark to HD number as: 0 = normal star 1 = A component, 2 = B component, etc 99 = combination of two consecutive HD numbers --- DM Durchmusterung identification with component number=2 the first two bytes identify the catalogue BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Durchmusterung .. = not in any Durchmusterung --- KS Number by Klare & Szeidl (1966) --- LSS Number from "Luminous Stars in the Southern Mily Way" by Stephenson & Sanduleak (1971) --- USN Number by Blanco et al. (1970) --- LID Mermilliod (1978) Code number number=6 the Numeration Code introduced by Mermilliod (1978) was extended with the following numbers: 4.12AABBBB Star BBBB in cluster Dol AA by Moffat et al. (1979) 6.003BBBBB Blanco et al (1970) 6.1007BBBB Hiltner W.A.: 1956, ApJS 2, 389 6.1008BBBB Merill P.W., Burwell C.G.: 1949, ApJ 110, 387 6.1009BBBB Klare & Szeidl (1966) Neckel Th.: 1967, Veroeff. Landessternwarte Heidelberg-Koenigstuhl Vol.19 6.20027BBB Merill P.W., Burwell C.G.: 1950, ApJ 112, 72 Merill P.W., Burwell C.G.: 1933, ApJ 78, 87 Merill P.W., Burwell C.G.: 1943, ApJ 98, 153 6.20028BBB Muench L.: 1956, Bol. Inst. Tonantzintla 2 No14, 35 6.20029BBB Slettebak A., Bahner K., Stock J.: 1961, ApJ 134, 195 6.20030BBB Gonzales G., Gonzales G.: 1955, Bol. Inst. Tonantzintla 2 No13, 3 Gonzales G., Gonzales G.: 1954, Bol. Inst. Tonantzintla 2 No11, 25 Gonzales G., Gonzales G.: 1954, Bol. Inst. Tonantzintla 1,No9, 3 6.20032BBB Whiteoak J.B.: 1962, MNRAS 125, 105 6.20033BBB Muench G. Muench L.: 1964, ApJ 140, 162 6.20037BBB Goy G.: 1973, A&AS 12, 277 6.20038BBB Bigay J.H., Garnier R., Georgelin Y.P.: 1972, A&A 18, 301 6.20039BBB Drilling J.S.: 1972, AJ 77, 463 6.20040BBB Neckel Th.: Heidelberg, Preliminary star numbers 6.309XXBBB Iriarte B., Chavaria E.: 1955, Bol. Inst. Tonantzintla 2 No13, 12 6.46803BBB Westerlund B.: 1963, MNRAS 127, 71 6.47301BBB Roslund C.: 1963, Arkiv for Astron. 3, 357 6.50AAA0BB Star BB in Sharpless region AAA by Moffat et al. (1979) 6.51AAA0BB Star BB in HII-region PM AAA by Moffat et al. (1979) 6.52AAA0BB Star BB in HII-region Wat AAA by Moffat et al. (1979) 6.53AAA0BB Star BB in HII-region RCW AAA by Moffat et al. (1979) 6.54AAA0BB Star BB in HII-region Anon. Moffat AAA by Moffat et al. (1979) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAcs Right Ascension 1950 (centi-seconds) 0.01s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg MKLum MK Luminosity Class number=3 The code for luminosity class is defined as follows: 10 = Ia 11 = Iab 12 = Ib 13 = I 15 = Ia+ 17 = Ib-II 20 = II 25 = II-III 30 = III 35 = III-IV 40 = IV 45 = IV-V 50 = V 60 = no luminosity class known only for O stars (Mk type classified from slit spectra) or luminosity class V assumed for derivation of the "photometric Mk type", if no beta-value is known. 70,71,72 apparently used for Wolf-Rayet, WC and WN stars 88 = galactic cluster (temperature class is always 0) 99 = delta Cep star (temperature class is always 990) --- MKTemp MK Temperature Class number=4 The code for temperature class is C*100+subdivision, where C = 0 : O-type (or Wolf-Rayet stars when luminosity class is 70,71 or 72) C = 1 : B-type C = 2 : A-type C = 3 : F-type C = 9 : only delta Cep star (associated to luminosity class is 99) Example: 115 means: B1.5 --- MKrem1 MK peculiarity number=5 The code for spectral peculiarities is defined as follows: 06 = MK: or (MK) 07 = n 08 = e 09 = p 17 = (n) 18 = (e) 19 = (p) 26 = MK:: 27 = nn 28 = e! 29 = p! 30 = f 31 = k 32 = ? 33 = var. example: 270908 means "nnpe" --- MKrem2 MK peculiarity number=5 The code for spectral peculiarities is defined as follows: 06 = MK: or (MK) 07 = n 08 = e 09 = p 17 = (n) 18 = (e) 19 = (p) 26 = MK:: 27 = nn 28 = e! 29 = p! 30 = f 31 = k 32 = ? 33 = var. example: 270908 means "nnpe" --- MKrem3 MK peculiarity number=5 The code for spectral peculiarities is defined as follows: 06 = MK: or (MK) 07 = n 08 = e 09 = p 17 = (n) 18 = (e) 19 = (p) 26 = MK:: 27 = nn 28 = e! 29 = p! 30 = f 31 = k 32 = ? 33 = var. example: 270908 means "nnpe" --- MKrem4 MK peculiarity number=5 The code for spectral peculiarities is defined as follows: 06 = MK: or (MK) 07 = n 08 = e 09 = p 17 = (n) 18 = (e) 19 = (p) 26 = MK:: 27 = nn 28 = e! 29 = p! 30 = f 31 = k 32 = ? 33 = var. example: 270908 means "nnpe" --- refMK Reference of Temperature Class (file refs) --- MKLum(ph) MK Photometric Luminosity Class number=3 The code for luminosity class is defined as follows: 10 = Ia 11 = Iab 12 = Ib 13 = I 15 = Ia+ 17 = Ib-II 20 = II 25 = II-III 30 = III 35 = III-IV 40 = IV 45 = IV-V 50 = V 60 = no luminosity class known only for O stars (Mk type classified from slit spectra) or luminosity class V assumed for derivation of the "photometric Mk type", if no beta-value is known. 70,71,72 apparently used for Wolf-Rayet, WC and WN stars 88 = galactic cluster (temperature class is always 0) 99 = delta Cep star (temperature class is always 990) --- MKTemp(ph) MK Photometric Temperature Class number=4 The code for temperature class is C*100+subdivision, where C = 0 : O-type (or Wolf-Rayet stars when luminosity class is 70,71 or 72) C = 1 : B-type C = 2 : A-type C = 3 : F-type C = 9 : only delta Cep star (associated to luminosity class is 99) Example: 115 means: B1.5 --- Vmag Photometric data from literature mag B-V Photometric data from literature mag U-B Photometric data from literature mag Vmag(H) Heidelberg photometric measurement mag B-V(H) Heidelberg photometric measurement mag U-B(H) Heidelberg photometric measurement mag Beta H-beta from the literature mag Beta(H) Heidelberg H-beta measurement mag r(MK) Distance from UBV+MK kpc r(Beta) Distance from UBV+beta kpc Av(MK) Extinction from UBV+MK mag Av(beta) Extinction from UBV+beta mag ref_UBV Reference for UBV (file refs) --- r_Beta Reference for beta (file refs) --- Francois Ochsenbein CDS 1995 Feb 07 UNKNOWN UNKNOWN * 07-Feb-1995(CDS): DM numbers, right ascension, declination, spectral peculiarities have been converted from the original values. Notes, remarks, references have been added using the printed documentation. II_62.xml A Catalogue of observations in H alpha 2066 II/66 A Catalogue of observations in H alpha A Catalogue of observations in H alpha J R Ducati Astron. Astroph. Suppl. 45 119 1981 1981A&AS...45..119D Photometry, H-alpha Equivalent widths This catalogue contains 4095 published observations of the quantitative observations of H{alpha} for 2700 stars. These observations were collected from values published between 1949 and 1980. The H{alpha} index was reduced to a common system described by Strauss & Ducati (1981A&AS...44..337S); the values of the original index can be retrieved with a linear transformation (cc = correlation coefficient): ----------------------------------------------------------------- References a b cc lower upper Spectral range ----------------------------------------------------------------- 2 1.401 -1.604 0.972 1.050 1.170 10 1.33 -2.4 0.000 13 1.526 0.130 0.992 2.910 3.300 14,36 0.343 0.814 0.949 1.400 O B A0 14,36 0.269 0.969 0.972 1.470 A1 F G K M 20,21,22,23,37 0.39 -0.55 1.200 24,25 1.35 -1.48 0.922 1.020 1.170 -----------------------------------------------------------------
Published measurements HD Star identification, usually HD --- m_HD HD suffix (/3,/0, A, B, etc.) --- ID Alternate designation --- Sp Spectral type from original reference --- Vmag Visual magnitude if provided mag Ha H alpha measurement --- u_Ha Uncertainty code for H alpha --- e_Ha Mean error of H alpha measurement --- x_Ha Method of measurement of Ha M = photoelectric photometry, value given in magnitudes. W = data from microdensitometer tracings of stellar spectra R = spectrophotometric measurements, where R = H-alpha ratio --- o_Ha Number of observations or weight --- w_wt Weight of weight --- rem Coded remarks 1 = Variable star 2 = Possible variable star 3 = Emission, mainly Be or Ae stars 4 = Double or multiple system 5 = Standard star 6 = Mean value over several measurements --- ref Reference number (file refs.dat) --- Homogeneous data ID HD number or other name --- Ha H-alpha index on common system (see Strauss & Ducati, 1981A&AS...44..337S) mag ref References to original data --- References in numerical order ref Reference number --- Cont Continuation --- source Text of reference --- Nancy G. Roman ADC/SSDOO rev. F. Ochsenbein CDS 1995 Aug 15 II_66.xml OAO 2 Ultraviolet Photometry: An Atlas of Stellar Spectra 2067 II/67 OAO-2 Ultraviolet Photometry, Stellar Spectra OAO 2 Ultraviolet Photometry: An Atlas of Stellar Spectra M R Meade A D Code Astrophys. J. Suppl. 39 195 1979 1979ApJS...39..195M OAO 2 Ultraviolet Photometry: An Atlas of Stellar Spectra M R Meade A D Code Astrophys. J. Suppl. 42 283 1980 1980ApJS...42..283M Photometry, ultraviolet Spectrophotometry The catalog is a subset comprising the highest quality data obtained with both spectrometers aboard the Orbiting Astronomical Observatory (OAO 2). The original catalog dealt with three data files. The first file contained ultraviolet stellar fluxes for 164 bright stars in the spectral region 1200-3600 angstroms with resolutions of 22 angstroms in the region from 3600 to 1850 angstroms and 12 angstroms in the region from 1850 to 1160 angstroms. Files 2 and 3 contained spectra for 132 stars in the region 1200-1850 angstroms and 34 stars in the region 1800-3600 angstroms, respectively, with resolutions as stated above. The monochromatic flux is given in units of erg/cm2/sec/angstrom for all data. The data have been published in graphical and tabular form in the cited papers. For data analysis and plotting purposes, we re-formatted the original files so that each data file represents the result (the wavelength and flux) for each star.
OAO-2
Catalog data for Zeta Puppiss Catalog data for S Monocerotis Catalog data for Xi Persei Catalog data for HR 5680 Catalog data for Lambda Orionis Catalog data for 68 Cygni Catalog data for 10 Lacertae Catalog data for Iota Orionis Catalog data for Zeta Orionis Catalog data for HR 7589 Catalog data for Alpha Camelopardi Catalog data for 19 Cephei Catalog data for Mu Columbae Catalog data for Sigma Orionis Catalog data for Delta Orionis Catalog data for Zeta Orionis Catalog data for Upsilon Orionis Catalog data for Tau Scorpii Catalog data for Epsilon Orionis Catalog data for Theta Muscae Catalog data for Kappa Orionis Catalog data for Epsilon Persei Catalog data for Beta Crucis Catalog data for Lambda Leporis Catalog data for Alpha 1 Crucis Catalog data for Phi 1 Orionis Catalog data for Gamma Cassiopeiae Catalog data for Delta Scorpii Catalog data for Eta Orionis Catalog data for Beta Scorpii Catalog data for 139 Tauri Catalog data for Zeta Persei Catalog data for Beta Canis Majoris Catalog data for Xi 1 Canis Majoris Catalog data for Sigma Scorpii Catalog data for Beta Cephei Catalog data for Epsilon Centaruri Catalog data for Beta Centauri Catalog data for Alpha Virginis Catalog data for VV Orionis Catalog data for 25 Orionis Catalog data for Pi Scorpii Catalog data for 60 Cygni Catalog data for Alpha Luporis Catalog data for Kappa Scorpii Catalog data for Lambda Scorpii Catalog data for Mu 1 Scorpii Catalog data for Eta Centauri Catalog data for 1 Scorpii Catalog data for Eps Canis Majoris Catalog data for Gamma Orionis Catalog data for HR 6143 Catalog data for Beta Lupi Catalog data for Zeta Cassiopeiae Catalog data for Gamma Pegasi Catalog data for Omega Orionis Catalog data for Mu 2 Scorpii Catalog data for Nu Centauri Catalog data for Rho Scorpii Catalog data for Phi Centauri Catalog data for Upsilon 1 Centauri Catalog data for Epsilon Luporis Catalog data for 13 Scorpii Catalog data for Mu Centauri Catalog data for 22 Scorpii Catalog data for Zeta Canis Majoris Catalog data for Phi Persei Catalog data for Upsilon Cygni Catalog data for Zeta Centauri Catalog data for Eta Luporis Catalog data for Gamma Columbae Catalog data for Omega 1 Cygni Catalog data for Iota Luporis Catalog data for Xi Orionis Catalog data for Nu Orionis Catalog data for Eta Aurigae Catalog data for Eta Ursa Majoris Catalog data for Alpha Eridani Catalog data for Beta Monocerotis Catalog data for Zeta Tauri Catalog data for HR 4140 Catalog data for Lambda Crucis Catalog data for Delta Persei Catalog data for Eta Canis Majoris Catalog data for Tau Herculis Catalog data for Omicron Luporis Catalog data for 57 Cygni Catalog data for Nu Andromedae Catalog data for HR 5378 Catalog data for Zeta Draconis Catalog data for Beta Tauri Catalog data for Alpha Gruis Catalog data for Alpha Leonis Catalog data for Phi Andromedae Catalog data for Phi Sagitarii Catalog data for Beta Orionis Catalog data for Omega Carinae Catalog data for Nu Puppis Catalog data for Beta Persei Catalog data for Iota Andromedae Catalog data for Zeta Pegasi Catalog data for Alpha Andromedae Catalog data for Alpha Pegasi Catalog data for Zeta Aquilae Catalog data for Theta Aurigae Catalog data for Delta Cygni Catalog data for Phi Draconis Catalog data for Alpha Doradus Catalog data for Beta Carinae Catalog data for Gamma Geminorum Catalog data for Alpha Lyrae Catalog data for Alpha Coronae Borealis Catalog data for Gamma Trianguli Catalog data for Alpha Canis Majoris Catalog data for Beta Ursae Majoris Catalog data for Alpha Geminorum Catalog data for Alpha Cygni Catalog data for Beta Aurigae Catalog data for Alpha Piscis Austrini Catalog data for Beta Leonis Catalog data for Alpha Ophiuchi Catalog data for Beta Arietis Catalog data for Delta Cassiopeiae Catalog data for Gamma Bootis Catalog data for Alpha Leporis Catalog data for Alpha Carini Catalog data for Alpha Cephei Catalog data for Alpha Aquilae Catalog data for Theta Scorpii Catalog data for Beta Cassiopeiae Catalog data for Iota 1 Scorpii Catalog data for Sigma Bootis Catalog data for Alpha Ursae Minoris Catalog data for Alpha Canis Minoris Catalog data for Alpha Trianguli Catalog data for Chi Draconis Catalog data for Gamma Cygni Catalog data for Theta Draconis Catalog data for Eta Aquilae Catalog data for Beta Aquarii Catalog data for Beta Leporis Catalog data for Eta Bootis Catalog data for Zeta Herculis Catalog data for Beta Hydri Catalog data for Beta Draconis Catalog data for Alpha Centauri Catalog data for Epsilon Geminorum Catalog data for Zeta Cygni Catalog data for Delta Draconis Catalog data for Eta Draconis Catalog data for Alpha Aurigae Catalog data for Beta Herculis Catalog data for Alpha Cassiopeiae Catalog data for Epsilon Cygni Catalog data for Alpha Ursae Majoris Catalog data for Eta Cephei Catalog data for ALpha Bootis Catalog data for Alpha Arietis Catalog data for Alpha Tauri Catalog data for Alpha Orionis Catalog data for Beta Lyrae Catalog data for Gamma Velorum Catalog data for Alpha Scorpii Catalog data for HR 2583 Catalog data for HD 93131 Catalog data for UW Canis Majoris Catalog data for HR 6245 Catalog data for Delta Circini Catalog data for Tau Canis Majoris Catalog data for Mu Normae Catalog data for HR 3055 Catalog data for HR 3476 Catalog data for HR 3090 Catalog data for Kappa Aquilae Catalog data for Delta Pictoris Catalog data for 1 Cassiopeiae Catalog data for Theta Carinae Catalog data for Kappa Cassiopeiae Catalog data for Pho Leonis Catalog data for Gamma Arae Catalog data for Omicron Persei Catalog data for 15 Canis Majoris Catalog data for 40 Persei Catalog data for HR 1595 Catalog data for HR 1886 Catalog data for 42 Orionis Catalog data for Omega 1 Scorpii Catalog data for Sigma Cassiopeiae Catalog data for Pi Aquarii Catalog data for HR 3294 Catalog data for DD Lacertae Catalog data for Delta Lupi Catalog data for Kappa Canis Majoris Catalog data for HR 1423 Catalog data for Chi Ophiuchi Catalog data for 68 Herculis Catalog data for Epsilon Cassiopeiae Catalog data for Pi 4 Orionis Catalog data for Pi 5 Orionis Catalog data for Sigma Lupi Catalog data for Delta Ceti Catalog data for Kappa Centauri Catalog data for Gamma Lupi Catalog data for Theta Ophiuchi Catalog data for Upsilon Scorpii Catalog data for 6 Lacertae Catalog data for EW Lacertae Catalog data for Del Centauri Catalog data for Nu Scorpii Catalog data for Delta Caeli Catalog data for Omega Canis Majoris Catalog data for HR 2770 Catalog data for Kappa Velorum Catalog data for Alpha Muscae Catalog data for 10 Moncerotis Catalog data for HR 2787 Catalog data for Chi Centauri Catalog data for HR 2142 Catalog data for Alpha Arae Catalog data for 66 Ophiuchi Catalog data for HR 7807 Catalog data for Pi 2 Cygni Catalog data for Eta Lyrae Catalog data for Xi Cassiopeiae Catalog data for HR 2961 Catalog data for HR 3084 Catalog data for Tau Librae Catalog data for Lambda Librae Catalog data for Theta 1 Sagitarii Catalog data for Alpha Pavonis Catalog data for Epsilon Carinae Catalog data for HR 985 Catalog data for 2 Scorpii Catalog data for Theta Lupi Catalog data for Epsilon Capricorni Catalog data for Omicron 2 Canis Majoris Catalog data for Iota Canis Majoris Catalog data for 27 Canis Majoris Catalog data for Alpha Telescopii Catalog data for Sigman Sagitarii Catalog data for AR Cassiopeiae Catalog data for Chi Carinae Catalog data for 35 Arietis Catalog data for Tau Tauri Catalog data for HR 5471 Catalog data for Lambda Lupi Catalog data for Iota Herculis Catalog data for Phi 2 Lupi Catalog data for 67 Ophiuchi Catalog data for 3 Centauri Catalog data for 48 Librae Catalog data for Kappa Eridani Catalog data for 16 Puppis Catalog data for Pi Andromedae Catalog data for Rho Lupi Catalog data for Pi Lupi Catalog data for Zeta Sculptoris Catalog data for Psi Persei Catalog data for 2 Lacertae Catalog data for Theta Coronae Borealis Catalog data for Beta Piscis Catalog data for Omicron Andromedae Catalog data for Alpha Columbae Catalog data for Zeta Phoenicis Catalog data for HR 8535 Catalog data for Aplha Sculptoris Catalog data for HR 1063 Catalog data for Gamma Corvi Catalog data for Gamma Gruis Catalog data for Beta Canis Minoris Catalog data for Beta Librae Catalog data for Mu Ophiuchi Catalog data for 41 Eridani Catalog data for Upsilon Herculis Catalog data for Phi Herculis Catalog data for Lambda Centauri Catalog data for Gamma Lyrae Catalog data for Mu Leporis Catalog data for Epsilon Sagitarii Catalog data for Kappa Lupi Catalog data for Delta Corvi Catalog data for Lambda Aquilae Catalog data for Theta Aquilae Catalog data for Theta Hydrae Catalog data for Alpha 2 Canum Venaticorum Catalog data for 36 Luncis Catalog data for Epsilon Ursae Majoris Catalog data for Tau 9 Eridani Catalog data for Gamma Centauri Catalog data for Delta Velorum Catalog data for Gamma Ursae Majoris Catalog data for Zeta Sagitarii Catalog data for Zeta Ursae Majoris Catalog data for Eta Ophiuchi Catalog data for Beta Eridani Catalog data for Alpha 2 Librae Catalog data for HR 2467 Catalog data for HR 8023 Catalog data for Lambda Cephei Catalog data for HD 192163 Catalog data for HD 193793 Catalog data for HR 2422 Catalog data for HD 45314 Catalog data for HR 7767 Catalog data for P Cygni Catalog data for HR 7678 Catalog data for HR 8119 Catalog data for HR 7567 Catalog data for 3 Geminorum Catalog data for HR 7210 Catalog data for 6 Cephei Catalog data for HR 5358 Catalog data for Epsilon Doradus Catalog data for HR 2231 Catalog data for Nu Doradus Catalog data for Eta 1 Doradus Catalog data for Sigma Cygni Catalog data for Mu Orionis Catalog data for Delta Hydri Catalog data for Theta Geminorum Catalog data for Kappa Phoenicis Catalog data for Zeta Leporis Catalog data for Beta Trianguli Catalog data for Beta Pictoris Catalog data for Mu Andromedae Catalog data for Aplha Pictoris Catalog data for Iota Cugni Catalog data for Delta Doradus Catalog data for Epsilon Aurigae Catalog data for Theta Centauri lambda Wavelength nm flux Flux data in units of ergs cm-2s-1A-1 If a data point is 0.0, no measurement was made at that wavelength or no data was presented because of large uncertainty in the measurement. --- flag quality of the flux data A "+" sign indicates spectrometer 1 data otherwise spectrometer 2 data are assumed. An asterisk "*" after 0.0 stands for sigma/F is >= 20% and no data are presented (see Code and Meade 1979, p. 199). --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Apr 20 UNKNOWN UNKNOWN Unidentified numbers of the object identification are BS (=HR) identifications from the Yale Catalogue of Bright Stars (Hoffleit 1964). A magnetic tape containing the OAO 2 spectrometer data was received from Arthur D. Code on 19 August 1980. The tape was formatted as a print tape having the record structure and spacing of the printed pages in the Code and Meade (1979) and Meade and Code (1980) papers. Due to the programming complications arising from the original format, which contains blank lines and data for many stars within each logical record, it was decided to convert the tape to a more suitable format for data analysis and plotting purposes. Thus, the original format in the tape was converted to the format described in this document. II_67.xml Dearborn Observatory Catalogue of faint red stars 2068 II/68 Dearborn Catalogue of faint red stars Dearborn Observatory Catalogue of faint red stars O J Lee R J Baldwin D W Hamlin Ann. Dearborn Obs., vol. V, part 1A ??? ??? 1943 1947AnDea...1....5L Dearborn Observatory Catalogue of faint red stars O J Lee T J Bartlett Ann. Dearborn Obs., vol. V, part 1B ??? ??? 1944 1947AnDea...1....5L Dearborn Observatory Catalogue of faint red stars O J Lee G D Gore T J Baldwin Ann. Dearborn Obs., vol. V, part 1C ??? ??? 1947 1947AnDea...1....5L Stars, faint Stars, late-type The Dearborn Survey is the result of a survey of faint red stars conducted at the Dearborn Observatory from about 1932 to 1947. It covers the declination range -4.5deg to +90deg (54% of the Sky), and consisted of over 1800 direct plates and spectrograms carrying single or multiple exposures varying from a second to 4 hours. The magnitudes in the catalog were obtained from direct plates mostly sensitive in the 0.55-0.64{mu}m wavelength region. The spectral types were obtained from objective-prism plates with red-sensitive emulsion, and were classified on the visibility of the TiO bands.
The Dearborn Observatory catalog DO Dearborn number --- NoteFlag a note exists in the file "notes" the '#' indicates a note from the original catalogue, while the '*' indicates a note added at NASA Goddard Space Flight Center by Nagy (1979) --- RAh Right Ascension 1900 (hours) h RAm Right Ascension 1900 (minutes) min DE- Declination 1900 (sign) --- DEd Declination 1900 (degrees) deg DEm Declination 1900 (minutes) arcmin Rmag Magnitude on red-sensitive emulsion the magnitude was obtained through comparison with the International Polar Sequence; its accuracy was estimated to 0.2mag. mag n_Rmag Uncertainty and variability flag the following flags are used: * denotes an approximate value (parentheses around the magnitude in the published version) V for known variables ? for suspected variables --- SpType Dearborn spectral type --- HDtype Spectral type from HD (catalog <III/135>) only 5764 stars (13%) are in HD. --- Notes to the catalog DO Dearborn number --- Cont Indicates that there is a continuation in the next record --- Text Text of note --- Francois Ochsenbein CDS 1997 Jan 11 UNKNOWN UNKNOWN * August 1979 (Nagy, 1979): The Dearborn Observatory Catalogue of Faint Red Stars has been made machine-readable at the Goddard Space Flight Center and Wellesley College (Mrs. Sawyer, Whitin Observatory). All of the data in this catalogue has been keypunched, proofread and transferred to magnetic tape. * 11-Jan-1997: at CDS (Francois Ochsenbein), the declination of DO 1007 was corrected, and the original value of 99.9 Rmag reported for variables was changed to a 'V' flag. The notes mentioned in Nagy (1979) document were reported in the file "notes". This standardized document was added. UNKNOWN UNKNOWN Nomenclature Notes: Stars from this survey are designated sometimes as "DC" (Dearborn Catalogue) in the literature. The acronym "DO" (Dearborn Observatory) is recommended to designate the stars from this survey. II_68.xml Narrow-Band Photometry 2073 II/73 Narrow-Band Photometry Narrow-Band Photometry D H P Jones J E Sinclair J B Alexander Mon. Not. R. Astron. Soc. 194 403 1981 1981MNRAS.194..403J Photometry, narrow-band *** No Description Available ***
The catalog ID Star name --- RAh Right ascension hours (1950) h RAm Right ascension minutes (1950) m DE- Sign of declination --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin mag Magnitude at 7460 A mag e_mag Mean error of the magnitude cmag col1 Color: 6076 - 7460 A mag e_col1 Mean error of color 1 cmag col2 Color: 6830 - 7100 A mag e_col2 Mean error of color 2 cmag col3 Color: 7100 - 7460 A mag e_col3 Mean error of color 3 cmag Sp Spectral type --- r_mag Isource 1. Standard Star 3. Spectral type standard (Keenan 1963; Morgan & Keenan 1973; Wing 1973, 1978; Wing, Dean & MacConnell 1976 4. Trigonometric Parallax > 0.100 arcsec 5. Red star selected without consideration of its proper motion 6. Red star selected for its proper motion 7. Stars observed to relate the present observations with other photometric or spectrophotometric systems --- o_mag Number of observations --- N. G. Roman ADC/SSDOO 1997 Oct 03 II_73.xml Homogeneous catalogue of red and infrared magnitudes in the photoelectric photometric system of Kron 2075 II/75 Homegeneous RI magnitudes in Kron system Homogeneous catalogue of red and infrared magnitudes in the photoelectric photometric system of Kron G Jasniewicz Astron. Astrophys. Suppl. Ser. 49 99 1982 1982A&AS...49...99J II/8 : Catalogue of UVBGRI (system of Stebbins and Withford) data by Nicollier C. (Geneva Observatory) Magnitudes Photometry, infrared Photometry, Kron This catalogue (file "mean") contains homogeneous data in the photoelectric photometric system of Kron and Smith. The R magnitude and the R-I colour index have been collected from the literature published before January 1982. The homogenization method used in file "mean" has been described by Nicolet B. (1978, Astron. Astrophys. Suppl. 34,1).
R and R-I Measurements LID Lausanne designation number=1 The coded numbering system used in this catalogue has been described by Mermilliod J.-CL. (1978, Bulletin du Centre de Donnees Stellaires, Strasbourg,14,32). A minor modification consists in the suppression of the point for each code number. An eventual remark (such as multiplicity or variability) follows it. --- Rmag magnitude mag u_Rmag Uncertainty flag (:) on Rmag --- R-I Color index mag u_R-I Uncertainty flag (:) on R-I --- n_Nmes Note on measurements: S = Standard star / = Nmes does not appear * = Nmes is a minimum number --- Nmes Number of measurements --- Ref Reference --- R and R-I Homogeneous data LID Lausanne designation --- Rmag mean R magnitude mag R-I Mean colour index mag w_Rmag Weight on R colour --- w_R-I Weight on R-I index --- Ref1 First reference --- Ref2 Second reference --- Ref3 Third reference --- Ref4 Fourth reference --- First list of References Second list of References Ref Reference number; blank for continuation --- Text Text of reference --- Francois Ochsenbein CDS 1995 Sep 12 UNKNOWN UNKNOWN * January 1982: Magnetic tape provided to CDS by G. Jasniewicz * 04-Mar-1994: Catalogue documented at CDS (Francois Ochsenbein); the "code" file was added ; it is a strict copy of a similar file of 1986 from "UBV photometry catalogue" by Mermilliod J.C. (catalogue II/122) * 12-Sep-1995: "ReadMe" file completed. II_75.xml The Catalog of Non-Solar X-Ray Measurements 2077 II/77 Non-Solar X-Ray Measurements The Catalog of Non-Solar X-Ray Measurements J Arens R Rothschild NASA/GSFC Doc. X-661-75-230 ??? ??? 1975 1975 X-ray sources The catalog is a compilation of nearly all non-solar X-ray observations in the 0.1-500 keV range, reported by various observers. The catalog includes observer's institution, position in equatorial and galactic coordinates, source names, energy ranges of observations in keV, energy resolution in keV, temporal resolution, dates of observations, lengths of observations, types of detectors, vehicles carrying payload, references, comments of contributors, and background-type sources. As this catalog was published in September 1975, it is probably complete through 1974.
catalog data NUM List number --- acro_inst Acronyms of observing institutions ASE American Science and Engineering, Cambridge, Massachusetts BERK University of California, Berkeley, California BOLN Laboratorio TE.S.R.E. Bologna, Italy CASE Case-Western Reserve University, Cleveland, Ohio CIT California Institute of Technology, Pasadena, California COL Columbia University, New York, New York GSFC Laboratory for High Energy Astrophysics, Goddard Space Flight Center, Greenbelt, Maryland LEID Kamerlingh Onnes Laboratory, Leiden, The Netherlands LLL Lawrence Livermore Laboratory, Livermore, California LOCK Lockheed, Palo Alto Research Laboratory, Palo Alto, California LSPA Laboratory for Solar Physics and Astrophysics, Goddard Space Flight Center, Greenbelt, Maryland MIT Massachusetts Institute of Technology, Cambridge, Massachusetts NRL Naval Research Laboratory, Washinqton, D.C. RICE Rice University, Houston, Texas SCLY Saclay, France TATA Tata Institute, Bombay, India UCSD University of California, San Diego, California UHRU UHRU Satellite, American Science and Engineering, Cambridge, Massachusetts UNH University of New Hampshire, Durham, New Hampshire WISC University of Wisconsin, Madison, Wisconsin --- GLON Galactic longitude (decimal point in byte 14) all positions are UHURU positions unless specified otherwise in the comments (cf. bytes 550-556). deg GLAT Galactic latitude (decimal point in byte 21) all positions are UHURU positions unless specified otherwise in the comments (cf. bytes 550-556). deg Name Source name(s) --- Kev_range Energy range of observation (keV) --- Kev_res Energy FWHM resolution (keV) --- tempo_res Temporal resolution: S = seconds; MS = milliseconds; MMS = microseconds --- dat Date of observation (typically MM/DD/YY) --- exp_time Exposure time: S = seconds M = minutes; H = hours --- obs_area Effective area or geometry factor of observation (CM2 = cm2) --- DetType Detector type SCINT = scintillation counter GEIG CTR = geiger counter NAI = sodium iodide PROP CTR = proportional counter --- Vehicle Vehicle which carried payload: A = ANS (Astronomical Satellite of the Netherlands) B = balloon R = rocket U = UHURU satellite S/I = Saturn I Booster O/I = OSO I --- Ref Reference Astron and Astrophys Astronomy and Astrophysics Ap J The Astrophysical Journal Ap J. Suppl The Astrophysical Journal Supplement Astrophys Letters Astrophysics Letters Astrophys Space Sci Astrophysics and Space Science B.A.P.S. Bulletin of American Physical Society Can J P Canadian Journal of Physics 12th Cosmic Ray Conf. 12th International Cosmic Ray Conference GSFC Number GSFC PREPRINT (X-document) IAU Cir. IAU Circular JGR Journal of Geophysical Research Nature Nature Nat P S Nature, Physical Science New Tech. in Sp. Ast. New Techniques in Space Astronomy Nuovo Cim Nuovo Cimento Lett Nuovo Cim Nuovo Cimento Letters PRL Physical Review Letters Phys. Let. Physics Letters IAU Sym Proceedings of I.A.U. Symposium P.A.S.P. Publication of the Astronomy Society of the Pacific RSI Review of Scientific Instruments Science Science Solar Phys. Solar Physics Space Research Space Research Sp Sci Rev Space Science Review 5th Texas Symp on Rel. Astro. 5th Texas Symposium on Relativistic Astrophysics --- Note Comments of contributor --- BackType Background type source (no coordinates given for this class of source) --- RAh Equatorial coordinates (epoch 1950) Right ascension (decimal hours) h DEdeg Equatorial coordinates (epoch 1950) Declination (decimal degrees) deg equ_coord Source of equatorial coordinates Default source of equatorial coordinates is the UHURU satellite positions. Other position sources are as follows: (GC) General Catalogue of 33342 Stars for 1950., B. Boss (L) Detector entrance slit was perpendicular to the galactic plane and hence no resolution in galactic latitude (M) Messler Catalogue (PSR) D.O. Backer (private communication) (SNR) Ilovaisky and Lequenx SNR catalogue (3C) 3C Catalogue Revised (X) Position given by experimenter or in reference cited. --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Apr 10 UNKNOWN UNKNOWN The Catalog of Non-Solar X-Ray Measurements (Arens, J. and Rothschild, R. 1975 NASA/GSFC X-661-75-230) was received from Dr. R. Rothschild (NASA/GSFC Code 660) in October 1976. The version received had card image records with information on each entry. These card images were 80-byte records (the magnetic tape received had a blocksize of 16000 bytes) and totaled 2699 records (1301 entries). Each entry had a variable number of data cards associated with it (ranging from one to four), typically with 2 cards per entry where 12 entries had 4 cards. The input data segments of these card images were separated by a dollar sign ("$"). The published version of the catalogue (cf. reference above) did not define the number of entries in it, but a hand count results in 978 entries and the latest observation date appears to have been January 1975. Thus, the version presented here contains additional data (approximately 323 additional records and data at least as late as January 1976). The last record on the magnetic tape as received from Dr. R. Rothschild was a dummy 80 byte record with the value of 9999 as the counter to signal the end of the data set. This record has been dropped from the present version. A major deconvolution program (the major part of which was written by Mrs..Susan Ball) was written so as to assign the observational data into specific bytes so that the user can access the data in an efficient manner. The previous program (Code 660) used to process this data required reading all of the data into array areas in the program - so that as the data base grew, the program grew without bound. The new defined format presented here permits unlimited data and a small size program if the user chooses to list it in the same manner as the published catalogue. There were three types of coordinate data groups in the original data 1) entries having galactic coordinates 2) entries havinq equatorial coordinates 3) entries with no celestial coordinates, background For type one above, the equatorial coordinates at epoch 1950.0 were computed and added to the entry. For type two above, the galactic coordinates were computed and added to the entry. The background data entries are at the end of the data base since the tape is primary sorted by galactic coordinates with a secondary sort by catalogue list number. II_77.xml uvby-Beta Photometry of 398 Members of Visual Multiple Stellar Systems 2078 II/78 uvby-Beta Phot 398 Members of Visual Multiple Systems uvby-Beta Photometry of 398 Members of Visual Multiple Stellar Systems E H Olsen Astron. & Astrophys. Suppl. 48 165 1982 1982A&AS...48..165O Photometry, uvby, beta Stars, double and multiple The catalogue contains mainly two types of visual double stars: Evolved stars with main sequence companions; and systems, for which the IDS gives photometric and spectroscopic data, that suggest the secondary to be above the main sequence if the primary is placed on the main sequence. The photometry has been done with the Danish 50 cm reflector on La Silla, ESO, the limiting magnitude is 12m, separations are larger than 7". Identifications given are IDS, HD, and DM numbers. For each object V, b-y, ml, cl, and beta are given together with the number of nights, weights and r.m.s. errors of one observation (weight 1). The catalogue is published as table IV by E.H. Olsen, Astron. Astrophys. Suppl. 48, 165, where further details and discussion may be found.
uvby-beta photometry on standard visual double or multiple systems IDS IDS number The letters indicating individual components follow rigidly the IDS (Jeffers+ 1963) even in cases like IDS 17278S5534, where the A component is fainter than B. --- HD HD number --- rem Remark CPD = CPD number in DM / = Separates two numbers when star is composite --- DMsign Durchmusterung zone sign --- DMzone Durchmusterung zone --- DMnum Durchmusterung number in zone Durchmusterung numbers follow the convention of the HD catalogue: BD 1855 position North of declination -23deg CD South of above, and 1875 position North of -52deg CPD South of -52deg --- DMsuf Durchmusterung number suffix --- V V magnitude mag e_V RMS error on V mag b-y b-y color index mag e_b-y RMS error on b-y mag m1 m1 mag e_m1 RMS error on m1 mag c1 c1 mag e_c1 RMS error on c1 mag W1 Sum of Weights for uvby photometry Each observation was given weight 1 except in a number of cases where the difference in counting time was deemed to be so big that a weighting proportional to the counting time was thought more realistic. --- N1 Number of nights observed for uvby --- beta Beta index mag e_beta RMS error on beta mag W2 Sum of Weights for beta photometry Each observation was given weight 1 except in a number of cases where the difference in counting time was deemed to be so big that a weighting proportional to the counting time was thought more realistic. --- N2 Number of nights observed for beta --- Julie Anne Watko SSDOO/ADC 1996 Apr 10 The brief description above was written by Erik H. Olsen of the Copenhagen University Observatory. II_78.xml A Catalogue of Homogeneous Photometry of Bright Stars on the DDO System 2080 II/80 Homogeneous Photometry Bright Stars on DDO System A Catalogue of Homogeneous Photometry of Bright Stars on the DDO System R D McClure W T Forrester Publ. Dominion Astrophys. Obs. 15 439 1981 1981PDAO...15...14M Photometry, DDO Stars, bright The catalogue of homogeneous photometry of bright stars on the DDO (System McClure and Forrester 1981) is a compilation of DDO photometry of 2196 bright G and K stars prepared from observations made at Kitt Peak National and Cerro Tololo Inter-American Observatories over the last several years using filter sets well matched to the standard system. The catalogue includes a large number of DDO stars whose data have been taken directly from the standard-star paper of McClure (1976), plus a representative sample of stars selected from the Catalogue of Bright Stars (Hoffleit 1964) and the Catalogue of High-Velocity Stars (Eggen 1964) to have good velocities, spectral types and freedom from companion contamination. The catalogue contains HD Catalogue numbers, DM identifications; and the standard photometric indices of the DDO system: magnitude at 4800 angstroms, and the color indices c(45-48), c(42-45), c(41-42), c(38-41), and c(35-38). The number of observations from which each index was determined is also given, along with standard errors.
Catalog data cat Henry Draper (HD) Catalogue number (blank for five stars not in the HD) number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- flag1 HD Code (1 = A component; 9 if HD and HD+1 included in observation, e.g. 179957/8; 0 otherwise) number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- DM Durchmusterung catalog (DM) identification BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- sign Sign of DM zone number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- DMzon DM zone number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- DMnum DM number number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- m48 48 filter magnitude m48 number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag e_m48 Standard error sigma/sqrt(N) of m48 blank = no mean error given because of only a single observation, standard star, or error > 0.099 mag f_m48 Asterisk if error in m48 > 0.099 magnitude number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- C(45-48) Color-index C(45-48) number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag e_C(45-48) Standard error of C(45-48) number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mmag C(42-45) Color index C(42-45) number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag e_C(42-45) Standard error of C(42-45). See bytes 34-35. number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag C(41-42) Color index C(41-42) number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag e_C(41-42) Standard error of C(41-42). See bytes 34-35. number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag C(38-41) Color index C(38-41) number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag e_C(38-41) Standard error of C(38-41). See bytes 25-26. number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag f_C(38-41) Asterisk if error in C(38-41) > 0.099 number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- C(35-38) Color index C(35-38) number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag e_C(35-38) Standard error of C(35-38). See bytes 25-26. number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star mag f_C(35-38) Asterisk if error in C(35-38) > 0.099 number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- Nobs Number of observations Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- f_Nobs Note on Nobs * = Nobs is blank because number of observations is > 9 S = Standard star number= BD = Bonner Durchmusterung CD = Cordoba Durchmusterung CP = Cape Photographic Duchmusterung number= blank = no mean error given because of only a single observation, standard star, or error > 0.099 number= Array of 6 digits giving numbers of observations, Nobs, contributing to the magnitude and colors, respectively. Fields are all blanks for standard stars where data are taken directly from McClure (1976), and in cases where all Nobs > 9 (see byte 79). number= * = Nobs is blank because number of observations is > 9 S = Standard star --- M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1995 May 10 UNKNOWN UNKNOWN The catalogue was received on magnetic tape from Dr. Robert D. McClure of the Dominion Astrophysical Observatory on 5 January 1982. The following modifications to the original format were made in order to make the data easier to process by the general user while still retaining all information and coding in the original data set: 1. All records were condensed by eliminating unused bytes between the data fields in order to make room for the addition of Durchmusterung (DM) numbers for the HD stars. 2. DM numbers were inserted into the records by retrieving them from an updated and corrected version of the SAO-HD-DM-GC Cross Index (Warren and Roman 1981) which had been sorted by HD number. Eleven stars not in the cross index (non-SAO stars) were looked up manually using the HD catalogue and inserted. 3. Multiple HD numbers, e.g. HD 110379/80 were replaced by the lower number alone followed by a 9 to indicate that the data are for HD and HD + 1, i.e. the standard codes adopted by the Centre de Donnees Stellaires, Strasbourg, were added to all HD numbers (see description for byte 7). 4. Asterisks in the standard error fields of m48, C(38-41) and C(35-38), used to indicate errors > 0.099 mag, were moved to the flag bytes 27, 63 and 72 and those standard error fields were blanked out to allow the fields to be read with real format specifications. 5. Asterisks in the numbers of observations (Nobs) fields were converted to blanks and a single asterisk moved to byte 79 for the same reason as above. Also, the abbreviation "STD" in the Nobs fields was changed to blanks and the character "S" placed into byte 79 to flag standard stars. 6. Plus signs were added to all positive color-index data, always in the byte immediately preceding each datum. II_80.xml Catalog of Catalog of galactic O-type Stars 2082 II/82 Galactic O-type Stars Catalog of Catalog of galactic O-type Stars C D Garmany P S Conti C Chiosi Astrophys. J. 263 777 1982 1982ApJ...263..777G Stars, O The catalog is a compilation from the literature of all O-type stars for which spectral types, luminosity classes, and UBV photometry exist. The catalog contains 765 stars, for each of which designation (HD, DM, etc.), spectral type, V, B-V, absolute visual magnitude, absolute bolometric magnitude, cluster membership, distance, galactic coordinates, and source references are given. In addition, the authors have included derived values of absolute visual and bolometric magnitudes, and distances. The Catalog of Galactic O-Type Stars (Garmany, Conti and Chiosi 1982) is a compilation from the literature of all O-type stars for which spectral types, luminosity classes and UBV photometry exist. Most of the entries come from Cruz-Gonzalez, et al. (1974) and Humphreys (1978), with additional stars from Garrison and Kormendy (1976), Garrison, Hiltner and Schild (1977), Garrison and Schild (1979), Feinstein, Marraco and Muzzio (1973), Feinstein, Marraco and Forte (1976), and Moffat, FitzGerald and Jackson (1979).
Catalog of Galactic O-type stars ID Star identification Star identification: Henry Draper Catalogue (HD) number; Durchmusterung (DM) number; miscellaneous designations. Bytes 1-8 give the alphanumeric part of the catalog, cluster or miscellaneous designation; bytes 9-16 give the number of the star, and bytes 17-18 give component identifications where applicable. References for miscellaneous designations are: Designation Reference ------------ -------------------------------------------- GEORG Georgelin, Georgelin and Roux (1973). HILTNER Hiltner and Johnson (1956); Hiltner (1956). LS I Hardorp et al. (1959). LS II Stock et al. (1960). LS III Hardorp et al. (1964). LS IV Nassau and Stephenson (1963). LS V Hardorp et al. (1965). LS VI Nassau et al. (1965). LSS Stephenson and Sanduleak (1971). MILL Miller (1972). MART Martin (1967). S Sharpless (1959). ------------ -------------------------------------------- The format of the star identification field is entirely uniform within each type of identification, so the catalog can be sorted by name field and all HD, DM, NGC, etc. identifications will be ordered together properly. Alternate format specifications are given in parentheses. --- new_Sp New spectral type = * An asterisk (*) if the spectral type given is new and based upon either 63 A/mm or 79 A/mm spectra taken at Kitt Peak National Observatory. Blank if spectral type was taken from the literature. --- Sp Spectral Type Spectral type according to r_ID or r_Sp --- V V magnitude V, and B-V according to r_ID or r_Phot mag B-V B-V mag M(V) Absolute visual magnitude Absolute visual magnitude, M(V), taken from the primary source given in r_ID or from Conti's (1975) calibration of spectral type and M(V). mag Mbol Absolute bolometric magnitude Absolute bolometric magnitude computed using Conti's (1975) temperature scale and Morton's (1969) bolometric corrections as a function of temperature. mag Cl_mem Code for cluster or association membership Code for cluster or association membership, as listed below. Blank for presumed field stars. Code Group Code Group ---- ------------------------ ---- ----------------- 1 Sgr OB1 43 NGC 2129 2 Sgr OB7 44 Gem OB1 3 Sgr OB4 45 Mon OB1 4 Sgr OB6 46 Ori OB1 5 Ser OB1 47 Mon OB2 6 Sct OB3 48 CMa OB1 7 Ser OB2, NGC 6604 49 Cr 121 8 Sct OB2 50 NGC 2414 9 Cr 359 51 NGC 2362 10 Vul OB1 52 NGC 2439 11 Vul OB4 53 Pup OB1 12 Cyg OB3 54 Vel OB1 13 Cyg OB1 55 Car OB1 14 Cyg OB8 56 TR 14 15 Cyg OB9 57 TR 15 16 Cyg OB2 58 TR 16 17 Cyg OB4 59 Cr 228 18 Cyg OB7 60 Car OB2 19 NGC 6991 61 NGC 3576 20 Lac OB1 62 NGC 3766 21 Cep OB2, TR 37 nucleus 63 Cru OB1 22 Cep OB1 64 Cen OB1 23 NGC 7235 65 R 80 24 Cep OB5 66 Pis 20 25 Cep OB3 67 Nor OB1 26 Cas OB2 68 NGC 6067 27 Cas OB5 69 R 103 28 Cep OB4 70 R 105 29 Cas OB4 71 Ara OB1a 30 Cas OB14 72 NGC 6204 31 Cas OB7 73 Ara OB1b 32 Cas OB1 74 Sco OB1 33 NGC 457 75 Sco OB2 34 Cas OB8 76 HD 156154 group 35 Per OB1 77 M 6 36 Cas OB6 78 Sgr OB5 37 Cam OB1 79 zeta Pup 38 Per OB3 80 BO 4&5 39 Cam OB3 81 NGC 3572 40 Per OB2 82 Hogg 10 41 Aur OB1 83 Lynga 14 42 Aur OB2 84 NGC 6322 ---- ------------------------ ---- --- Dist Distance from star's distance modulus Distance computed from star's distance modulus, assuming an interstellar absorption of A(V)=3E(B-V). kpc GLONd Galactic longitude (whole degrees) The galactic longitude and lattitude are given in whole degrees and arc minutes rather than the frequently used decimal degrees. The sign of the Galactic lattitude is always in byte 68. deg GLONm Galactiv longitude (arc minutes) arcmin GLATd Galactic latitude; sign always in byte 68. deg GLATm Galactic latitude (arcmin) arcmin r_ID code for primary source The following list are references for the codes for primary source, additional cluster membership, additional spectral types, and additional photometry. The additional sources were generally used in cases where the data were missing or inadequate in the primary source or where there is disagreement among the papers consulted. Primary source (byte 75) Code Reference ---- --------------------------------------- 1 Cruz-Gonzalez et al. (1974). 2 Garrison, Hiltner and Schild (1977). 3 Humphreys (1978). 4 Garrison and Kormendy (1976). Garrison and Schild (1979). 5 Feinstein, Marraco and Muzzio (1973). Feinstein, Marraco and Forte (1976). 6 Moffat, FitzGerald and Jackson (1979). ---- --- r_Cl_mem code for additional cluster membership Additional cluster membership (byte 76) Code Reference ---- --------------------------------------- 1 Conti and Alschuler (1971). 2 Moffat and Vogt (1975). 3 Humphreys (1978). ---- --- r_Sp code for additional spectral types Additional spectral types (byte 77) Code Reference ---- --------------------------------------- 2 Garrison, Hiltner and Schild (1977). ---- --- r_Phot code for additional photometry, Additional photometry (byte 78) Code Reference ---- --------------------------------------- 4 Klare and Neckel (1977). 5 Feinstein, Marraco and Forte (1976). 6 Guetter (1974). ---- --------------------------------------- -------------------------------------------------------------- --- N.P.M. Kuin ADC 1994 Dec 10 Appreciation is expressed to C. D. Garmany for supplying the Catalog of Galactic O-Type Stars on magnetic tape with a listing and explanations, and for reviewing the modified catalog and resulting documentation. UNKNOWN UNKNOWN The Catalog of Galactic O-Type Stars was received on magnetic tape from Dr. C. D. Garmany of the University of Colorado on April 15, 1982. The following modifications were made to the format in order to make the star designations uniform (so that the file can be sorted by star name if desired) and to make the data records more homogeneous and easier to process by other users. 1.The B-V data were made uniform by attaching preceding zeros where they were not present and by moving minus signs so that they always occur in byte 65. 2.Minus signs for the bolometric magnitude field were moved in order to always occur in byte 47. 3.Cluster and association membership codes had been written as -0 if not present. These were changed to blanks. 4.Signs were attached to all Galactic latitude values, uniformly in byte 68. 5.Source codes of 0 were changed to blanks so that the string of codes in bytes 75-78 contains digits only where reference codes are present. 6.The star designation field was expanded to 18 bytes so that the identifications could be made uniform. The format was then changed by preparing a separate data set containing only the identifiers and editing all designations to contain catalog or cluster specifications in bytes 1-8, star numbers in bytes 9-16, and component identifications in bytes 17-18. The modified designation fields were then substituted back into the data file. A sort of the catalog by star designation will now yield a data set with all similar designations together and properly ordered. 7.The asterisk signifying a new spectral classification made by the authors, formerly appearing at the beginning of a record, was moved to byte 19. 8.Three duplicate entries were removed after carefully checking, confirming their redundancy, and notifying the first author. 9.The blanks in byte 48 and byte 69 were replaced by zero's. (1994/11/14) II_82.xml OAO2 filter Photometry of 531 stars of diverse types 2083 II/83 OAO2 filter Photometry of 531 stars OAO2 filter Photometry of 531 stars of diverse types A D Code A V Holm R L Bottemiller Astrophys. J. Suppl. Ser. 43 501 1980 1980ApJS...43..501C II/6 : Celescope Catalogue of Ultraviolet Magnitudes (Davis+ 1973) Berger, J. and Greenstein, J. L. 1963, Publ. Astron. Soc. Pac. 75, 336. (1963PASP...75..336B) Bernacca, P. L. and Molnar, M. R. 1972, Astrophys. J. 178, 189. (1972ApJ...178..189B) Code, A. D., Holm, A. V. and Bottemiller, R. L. 1980, Astrophys. J. Suppl. 43, 501 (1980ApJS...43..501C) Conti, P. S. and Smith L. F. 1972, Astrophys. J. 172, 623 (1972ApJ...172..623C) Cousins, A. W. J. 1971, Roy. Obs. Ann. No. 7. Cruz-Gonzalez, C. Recillas-Cruz, E., Costero, R., Peimbert, M. and Torres-Peimbert, S. 1974, Rev. Mexicana Astron. Astrofis. 1, 211. (1974RMxAA...1..211C) Greenstein, J. L. and Eggen, O. J. 1966, Vistas in Astronomy 8, 63. (1966VA......8...63G) Herbison-Evans, D., Hanbury-Brown, R., Davis, J. and Allen L. R. 1971, Mon. Not. R. Astron. Soc. 167, 121 (1971MNRAS.151..161B) Hiltner, W. A., Garrison R. F. and Schild R. E. 1969, Astrophys. J. 157, 313 (1969ApJ...157..313H) Hoffleit, D. 1964, Catalogue of Bright Stars (3rd ed., New Haven: Yale University Observatory) (see Cat. <V/50>) Holm, A. V. and Cassinelli, J. P. 1977, Astrophys. J. 211, 432. (1977ApJ...211..432H) Jaschek, C., Jaschek, M., Morgan, W. and Slettebak, A. 1968, Astrophys. J. (Letters) 153, L87 (1968ApJ...153L..87J) Jaschek, C., Hernandez, E., Sierra, A. and Gerhardt, A. 1972, Catalogue of Stars Observed Photoelectrically, Serie Astronomica, Vol. 38 (La Plata: University of La Plata). Jeffers, H. M., Van den Bos, W. H. and Greeby, F. M. 1963, "Index Catalogue of Visual Double Stars (IDS), Publ. Lick Obs. 21. Johnson, H. L., Mitchell, R. I., Iriarte, B. and Wisniewski, W. Z. 1966, Commun. Lunar and Planetary Lab. 4, 99 (Cat. <II/5>) Johnson, H. L. and Morgan W. W. 1953, Astrophys. J. 117, 313. (1953ApJ...117..313J) Joy, A. H. 1956, Asrophys. J. 124, 317 (1956ApJ...124..317J) Kukarkin, B. V., Kholopov, P. N., Pskovsky, Yu. P., Efremov, Yu. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Fedorovich, V. P. and Frolov, M. S. 1969, "General Catalogue of Variable Stars" (3rd ed., Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.). Lesh, J. R. 1968, Astrophys. J. Suppl. 17, 371 (1968ApJS...17..371L ; Cat. <II/23>) Molnar, M. R. 1974, Astrophys. J. 187, 531 (1974ApJ...187..531M) Morgan W. W. and Keenan, P. C. 1973, Ann. Rev. Astron. Astrophys. 11, 29 (1973ARA&A..11...29M) Photometry, ultraviolet The catalog contains the ultraviolet photometry of 531 stars observed with the Wisconsin Experiment Package aboard the Orbiting Astronomical Observatory (OAO-2). The data were obtained with medium-band interference filters and have been reduced to a uniform magnitude system. The ultraviolet magnitudes contained in the catalog have been published by Code et al. (1980). While the published tables contain 11 tabulated magnitudes, the machine version includes a twelfth filter (S2F2 at 2945 A). The catalog includes cross identifications to the numbering systems of the Bright Star Catalogue, The Henry Draper Catalogue, and the GC, star name, spectral type, V magnitude, B-V, U-B, references, remarks, and 12 ultraviolet magnitudes. The effective wavelengths (for a flat spectrum source) are 4250A, 3320A, 2980A, 2965A, 2460A, 2380A, 2035A, 1910A, 1680A, 1550A, 1430A, and 1330A. For most filters, the full width, half maximum is about 30% of the central wavelength.
OAO-2
The catalog (Table 2 of publication) HD Henry Draper Catalogue (HD) number <III/135> --- m_HD Additional HD number if > 1 HD star included --- HR Bright Star Catalogue (HR=BS) number <V/50> --- m_HR Additional HR number if > 1 HR star included --- Name Name of star --- SpType Spectral type from miscellaneous sources number=1 the spectral type contains in bytes: 25-26: luminosity class for Mt. Wilson types; W in byte 26 for W-R types 27-30: temperature class and subclass (generally uniform except that Q will be found for HD174107 = V603 Aql; N and C for W-R types) 31-37: additional spectral-type information; e.g., luminosity classes, abundance indicators, emission (e) and peculiar (p) symbols, and additional components (e.g. + dG5) --- Vmag V or visual magnitude from various sources (see also r_SpType) mag B-V B-V from various sources (see also r_SpType) mag U-B U-B from various sources (see also r_SpType) mag r_SpType Reference codes for spectral types and photometry number=2 References for Codes in Bytes 51-52: ------------------------------------------------------------------------ Spectral Types (byte 51) ------------------------------------------------------------------------ 1. Morgan and Keenan 1973ARA&A..11...29M 2. Johnson and Morgan 1953ApJ...117..313J 3. Hiltner, Garrison and Schild 1969ApJ...157..313H 4. Lesh 1968ApJS...17..371L (Cat. <II/23>) 5. Cruz-Gonzalez et al. 1974RMxAA...1..211C 6. Jaschek et al. 1972, "Cat. of Stars Observed Photoelectrically" 7. Berger and Greenstein 1963PASP...75..336B 8. Greenstein and Eggen 1966VA......8...63G 9. Joy 1956ApJ...124..317J 0. See file "notes.dat" for source ------------------------------------------------------------------------ UBV Photometry (byte 52) ------------------------------------------------------------------------ A. Johnson et al. 1966 (Cat. <<II/5>) B. Cousins 1971, Roy. Obs. Ann. No. 7 C. Johnson and Morgan 1953ApJ...117..313J D. Cruz-Gonzalez et al. 1974RMxAA...1..211C E. Jaschek et al. 1972, "Cat. of Stars Observed Photoelectrically" F. Berger and Greenstein 1963PASP...75..336B O. See file "notes.dat" for source --- Rem Remarks codes number=3 See details in Table 3 below. Codes are for remarks pertaining to: D for visual double or multiple system, SB for spectroscopic binary, V for variable, and * for miscellaneous remarks. --- m4250 Magnitude at 4250 / mag u_m4250 Colon (:) for uncertain data --- m3320 Magnitude at 3320 / mag u_m3320 Colon (:) for uncertain data --- m2980 Magnitude at 2980 / mag u_m2980 Colon (:) for uncertain data --- m2945 Magnitude at 2945 / mag u_m2945 Colon (:) for uncertain data --- m2460 Magnitude at 2460 / mag u_m2460 Colon (:) for uncertain data --- m2380 Magnitude at 2380 / mag u_m2380 Colon (:) for uncertain data --- m2035 Magnitude at 2035 / mag u_m2035 Colon (:) for uncertain data --- m1910 Magnitude at 1910 / mag u_m1910 Colon (:) for uncertain data --- m1680 Magnitude at 1680 / mag u_m1680 Colon (:) for uncertain data --- m1550 Magnitude at 1550 / mag u_m1550 Colon (:) for uncertain data --- m1430 Magnitude at 1430 / mag u_m1430 Colon (:) for uncertain data --- m1330 Magnitude at 1330 / mag u_m1330 Colon (:) for uncertain data --- Notes to catalog ID Designation of the star, generally HD, repeated when several lines are required. --- Text Text of remark --- Francois Ochsenbein CDS 1998 Apr 15 We express our appreciation to M. R. Meade of the Space Astronomy Laboratory, University of Wisconsin, for supplying the original magnetic tape and format description, and to A. V. Holm for reviewing this document. UNKNOWN UNKNOWN * From Wayne H. Warren, January 1982, NSSDC/WDC-A-R&S 82-02: The Catalog of OAO 2 Filter Photometry was received on magnetic tape from the Space Astronomy Laboratory, University of Wisconsin, in August 1981. A format description of the Wisconsin tape and a listing of the tape contents were received simultaneously. The following modifications were made to the catalog format in order to save storage space and to make the records easier to process: 1. The Wisconsin tape contained two card images (160 bytes) per star. Elimination of unused bytes and sequence numbers assigned to the original observed objects, and merging of the card images to a single logical record per star resulted in the present 132-byte record length. 2. HD and HR numbers were left justified in the catalog as received. They were converted to right justified integers so that they can be read properly with an integer format specification. 3. The spectral types field was expanded from 11 bytes to 13 bytes (to allow for spacing and uniformity) and temperature classes and subclasses always occur in bytes 27 and 28-30, respectively. The Mt. Wilson and W (Wolf- Rayet) prefixes were moved so that they always occur in bytes 25-26 (the Mt. Wilson luminosity types and other normally lower case characters have been converted from upper to lower case). The spectral type for HD197989 (e Cyg), which is K0- III, was changed from K0 III to K0 -III. 4. The HD number for V1357 Cyg (Cyg X-1) was changed from E226868 to 226868 to eliminate the character from the HD field and to make it uniform. Certain Durchmusterung numbers, which were incomplete, were completed and made uniform within the star name field. 5. One byte following each ultraviolet magnitude field was preserved and those magnitudes having colons in Table 2 of Code, Holm and Bottemiller (1980) were appended with colons in the machine-readable catalog. * 15-Apr-1998: File notes.dat prepared at CDS. II_83.xml 13-color Photometry of 1380 Bright Stars 2084 II/84 13-color Photometry of 1380 Bright Stars 13-color Photometry of 1380 Bright Stars H L Johnson R I Mitchell Rev. Mex. Astron. Astrofis. 1 299 1975 1975RMxAA...1..299J Photometry, 13-color Stars, bright The catalogue contains observations of essentially all stars brighter than fifth visual magnitude north of declination -20 degrees and brighter than fourth visual magnitude south of declination -20 degrees, in the 13-color medium-narrow-band photometric system.
The 13-color photometry (Table 7) Remark '*' if remark number=3 Individual Notes: ------------------------------------------------------------------------ 215 Zet And 58 filters differ by more than 0.10 mag 681 Omi Cet 39831.6 matched to 39151.6 1239 Lam Tau 39873.6 matched to 39440.8 1845 CE Tau 39831.8 matched to 39499.7 2061 Alp Ori 39797.9 matched to 38787.7 2308 BL Ori 39773.9 matched to 39501.8 2590 Pi CMa 58 filters differ by more than 0.10 mag. May be variable. 2650 Zet Gem 39804.9 matched to 38789.8 4163 U Hya 58 filters differ by more than 0.10 mag. 33 was not measurable, 33-52=12 is a lower limit. 4846 Gam CVn 39867.9 matched to 39176.9. 33 was not measurable, 33-52=12 is a lower limit. 4915 Alp2 CVn 39930.7 matched to 38894.7 5056 Alp Vir 39930.8 matched to 39176.9 5589 RR UMi 39910.9 matched to 39257.8 6146 g Her 39969.8 matched to 38929.7 6406 Alp Her 39973.7 matched to 39227.9 6431 Mu Her 58 filters differ by more than 0.10 mag. 7066 R Sct 39974.9 matched to 38917.8 7564 Chi Cyg 40004.9 matched to 40006.9 (unpublished data) 7570 Eta Aql 39976.9 matched to 38871.9 8262 W Cyg 58 filters differ by more than 0.10 mag. 8297 V460 Cyg 33 was not measurable, 33-52=12 is a lower limit. 8316 Mu Cep 58 filters differ by more than 0.10 mag. 8383 VV Cep 58 filters differ by more than 0.10 mag. 8571 Del Cep 39278.8 matched to 39459.6 8752 HD 217476 58 filters differ by more than 0.10 mag. --- HR Harvard Revised (Bright Star) designation number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 --- Misc Miscellaneous info. re designation or physical characteristics number=1 Miscellaneous information regarding identification or physical characteristics; e.g. /X,/XX, -X for additional HR numbers included; 'V' or 'D' for variable or double star; '.' for uncertainty; '*' for 3 stars (HR4883, 6707, and 8143) but meaning is not defined in paper, nor could any common peculiar characteristics be found. --- SpType Spectral type number=2 Luminosity class for Mt. Wilson types; W in W-R types. Temperature class, subclass, and additional spectral-type information are listed. --- n_52 'X' if 52 magnitude from Cape V magnitude number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 --- 52 Magnitude, filter 52 number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 33-52 33 - 52 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 35-52 35 - 52 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 37-52 37 - 52 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 40-52 40 - 52 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 45-52 45 - 52 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 52-58 52 - 58 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 52-63 52 - 63 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 52-72 52 - 72 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 52-80 52 - 80 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 52-86 52 - 86 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 52-99 52 - 99 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag 52-110 52 - 110 color number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 mag Obs(Blue) Number of blue observations (filters 33 to 63) number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 --- Obs(Red) Number of red observations (filters 72 to 110) number= ---------------------------- Filter Effective Wavelength (Angstroems) ---------------------------- 33 3371 35 3536 37 3751 40 4030 45 4571 52 5183 58 5827 63 6356 72 7241 80 8000 86 8584 99 9831 110 11084 --- Francois Ochsenbein CDS 1995 Aug 30 UNKNOWN UNKNOWN * March 1981, by Wayne H. Warren Jr. and Nancy G. Roman at NASA/ADC (document NSSDC/WDC-A-R&S 81-02): "A magnetic tape version of the Thirteen-Color Photometry of 1380 Bright Stars was received from the Centre de Donnees Stellaires (CDS), Strasbourg (Identification Number 2052A78). As received, the spectral types had no uniformly coded fields for searching purposes, and no flags were included in the records to indicate remarks. In order to improve the uniformity of the spectral types, the entire catalogue was transferred from tape to disk at the Astronomical Data Center, and modifications were made interactively. The spectral types were modified such that the temperature class and subclass always occur in bytes 12 and 13, respectively. Mt. Wilson luminosity codes (g, d, sg, c, etc.) were shifted to occur uniformly in bytes 10-11, as was the W in each Wolf-Rayet type. Characters which are lower case in standard astronomical notation (e.g., Mt. Wilson luminosity codes, m and p in peculiar and metallic-line A stars, a, b, ab in luminosity classes, e for emission-line stars, etc.) were converted from upper to lower case. These characters should print as normal upper-case characters on conventional upper-case-only printers, but the use of an extended chain printer is suggested if one is available. The asterisks were also added as the remarks flag in byte 1 and the catalogue was transferred back to magnetic tape. A considerable number of stars had no MK types in the catalogue as received. When available, these types were added from the catalogues of M. Jaschek (1978), Kennedy (1978) and Morgan and Keenan (1973). Additional MK types were found for stars south of -40 degrees in Houk and Cowley (1975) and Houk (1978). Where possible, attempts were made to resolve uncertainties and to correct obvious errors. The order of the files (by HR number) is unchanged from the published catalogue (Johnson and Mitchell 1975), but they do differ slightly in that the star names present in the published catalogue (Table 7) have never been present on the disk." * October 1991: prepared by Lee E. Brotzman as files on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory /photom/13color * 30-Aug-1995: documentation from CD-ROM standardized at CDS; the SpType column has been enlarged to accommodate composite spectral types. II_84.xml Absolute Calibration of Stellar Spectrophotometry 2085 II/85 Absolute Calibration of Stellar Spectrophotometry Absolute Calibration of Stellar Spectrophotometry H L Johnson Rev. Mex. Astron. Astrofis. 5 25 1980 1980RMxAA...5...25J Spectrophotometry The catalog contains the absolute fluxes for 16 stars published in Tables 1 and 2 of Johnson (1980). The absolute calibrations were accomplished by combining the 13-color photometry calibrations of Johnson and Mitchell (1975) with spectra obtained with a Michelson spectrophotometer and covering the wavelength range 4000 to 10300 Angstroms (Johnson 1977). The agreement between the absolute calibration and another recent one based upon data for alpha Lyr and 109 Vir by Tug et al. (1977) is shown (Johnson 1980) to be quite good. The catalog includes star name, cross identifications to the numbering systems of the Bright Star Catalogue and The Henry Draper Catalogue and arrays of fluxes having the same number of elements for each of the 16 stars.
HR 875 HD 18331 (A1V) 02 56 37.5 -03 42 42 HR 1855 HD 36512 ups Ori (B0V) 05 31 55.8 -07 18 05 HR 2491 HD 48915 alf CMa (A1V) 06 45 10.8 -16 41 58 HR 3314 HD 71155 (A0V) 08 25 39.8 -03 54 22 HR 4534 HD 102647 bet Leo (A3V) 11 49 05.2 +14 34 25 HR 4662 HD 106625 gam Crv (B8III) 12 15 48.9 -17 32 32 HR 4942 HD 113791 xi2 Cet (B1.5V) 13 06 54.7 -49 54 21 HR 5511 HD 130109 109 Vir (A0V) 14 46 15.2 +01 53 36 HR 5685 HD 135742 bet Lib (B8V) 15 17 00.7 -09 22 57 HR 6629 HD 161868 gam Oph (A0V) 17 47 53.5 +02 42 30 HR 7001 HD 172167 alf Lyr (A0V) 18 36 55.4 +38 46 47 HR 7235 HD 177724 zet Aql (A0V) 19 05 24.5 +13 51 53 HR 7906 HD 196867 alf Del (B9IV) 20 39 38.0 +15 54 43 HR 8622 HD 214680 10 Lac (O9V) 22 39 15.6 +39 03 01 HR 8634 HD 214923 zet Peg (B8V) 22 41 27.4 +10 49 53 HR 8781 HD 218045 alf Peg (B9III) 23 04 45.4 +15 12 21
The Absolute fluxes of 16 stars lambda Wavelength 0.1nm F01 Flux for HR 7906 = HD 196867 = alf Del mW/m2/Hz F02 Flux for HR 5685 = HD 135742 = bet Lib mW/m2/Hz F03 Flux for HR 4662 = HD 106625 = gam Crv mW/m2/Hz F04 Flux for HR 6629 = HD 161868 = gam Oph mW/m2/Hz F05 Flux for HR 4942 = HD 113791 = xi2 Cet mW/m2/Hz F06 Flux for HR 7235 = HD 177724 = zet Aql mW/m2/Hz F07 Flux for HR 875 = HD 18331 mW/m2/Hz F08 Flux for HR 3314 = HD 71155 mW/m2/Hz F09 Flux for HR 2491 = HD 48915 = alf CMa mW/m2/Hz F10 Flux for HR 7001 = HD 172167 = alf Lyr mW/m2/Hz F11 Flux for HR 8781 = HD 218045 = alf Peg mW/m2/Hz F12 Flux for HR 4534 = HD 102647 = bet Leo mW/m2/Hz F13 Flux for HR 1855 = HD 36512 = ups Ori mW/m2/Hz F14 Flux for HR 8622 = HD 214680 = 10 Lac mW/m2/Hz F15 Flux for HR 5511 = HD 130109 = 109 Vir mW/m2/Hz F16 Flux for HR 8634 = HD 214923 = zet Peg mW/m2/Hz Francois Ochsenbein CDS 1997 Apr 29 UNKNOWN UNKNOWN The file was reformatted at CDS in 17 columns, one for the wavelength, and one for each star. The Description was added by Gail L. Schneider [SSDOO/ADC]. The positions and spectral types of the stars were added by F. Ochsenbein [CDS] II_85.xml Supplement to the Ultraviolet Bright Star Spectrophotometric Catalogue 2086 II/86 UV Bright-Star Spectrophotetric Supplement Supplement to the Ultraviolet Bright Star Spectrophotometric Catalogue D Macau-Hercot C Jamar A Monfils L Thompson L Houziaux R Wilson ESA Special Report 28 ??? ??? 1978 1978N79-16752.....M II/59 : Catalogue of stellar UV fluxes (TD1) (Thompson et al., 1978) III/39 : UV Bright Star Spectrophotometric Catalog (Jamar et al., 1976) Boksenberg A., Evans R.G., Fowler R.G., Gardner I.S.K., Houziaux L., Humphries C.M., Jamar C., Macau D., Malaise D., Monfils A., Nandy K., Thompson G.I., Wilson R., Wroe H., =1973MNRAS.163..291B Jamar C., Macau-Hercot D., Monfils A., Thompson G.I., Houziaux L., Wilson R., 1976, "Ultraviolet Bright Star Spectrophotometric Catalogue", ESA Special Report 27, =III/39A Thompson G.I., Nandy K., Jamar C., Monfils A., Houziaux L., Carnochan A., Wilson R., 1978, "Catalogue of stellar ultraviolet fluxes (TD1)", The Science Research Council, U.K., =II/59B Thompson G.I., Nandy K., Jamar C., Monfils A., Houziaux L., Carnochan A., Wilson R., 1979, =1979BICDS..17...78T, Catalog =V/38 Spectrophotometry Photometry, ultraviolet This catalogue is a supplement of the Ultraviolet Bright Star Spectrophotometric Catalogue (=III/39A). It contains observations carried out by the S2/68 Ultraviolet Sky Survey Telescope (UVSST) aboard the ESRO satellite TD-1. The data presented in this supplement were obtained during the second and third observation periods, which lasted from 19 February 1973 to 30 September 1973 and from 16 February to 6 May 1974. The S2/68 experiment has been described by Boksenberg et al. (=1973MNRAS.163..291B) Owing to the optical scanning mode, most of the stars observed during the first observational period, the spectra of which are included in the "Ultraviolet Bright-Star Spectrophotometric Catalogue", were seen again by the telescope. This supplement, however, has been limited to the spectra of stars that were not observed during the first period. The data reduction and selection criteria are identical to those underlying the main Catalogue and hence the data presented in the Supplement are directly comparable with those in the main Catalogue. The Supplement contains data for 435 stars. For a statistical summary of the observed stars, see the tables I and II in the published version of the Supplement. The spectrum scanning itself was achieved by the movement of a star image across the wide entrance slot of the spectrophotometer, which caused the corresponding spectrum image to pass over the three exit slits in the direction of dispersion. The motion of the primary image during each detector integration interval (0.148 s) was equivalent to 19.4 A, depending on the channel. The wavelength range covered was 1350 - 2550 A. The passband of the photometer channel, defined by a glass transmission filter and the photocathode tube response, was centered at 2740 A and had a full width at half height of 310 A.
TD 1A
The UV Spectrophotometric Supplement. RAh Right Ascension 1900 (hours) from HD h RAm Right Ascension 1900 (minutes) from HD min DE- Declination 1900 (sign) from HD --- DEd Declination 1900 (degrees) from HD deg DEm Declination 1900 (minutes) from HD arcmin HD designation --- Nsp Number of individual spectra that have been averaged --- F2740 Flux measured by the first photometer at 274nm (see TD1 Catalogue, Thompson et al., 1978) 10mW/m2/nm e_F2740 Mean error on F2740 % Fmax Highest flux for that star 10mW/m2/nm Flux UV fluxes at wavelengths from 135nm to 254nm, (1350-2540A), step 1nm(10A) (units are erg/cm2/s/Angstroem) 10mW/m2/nm e_Flux Error on Fluxes, in percent % Francois Ochsenbein CDS 1995 Oct 24 UNKNOWN UNKNOWN * The catalogue was provided to CDS by G.I. Thompson in 1979. * A CD-ROM version with most of the enclosed description section was created in October 1991 at ADC on the "Selected Astronomical Catalogs" Vol. 1 , directory /spectro/uvbssupp * 24-Oct-1995: the catalog was reformatted at CDS (Francois Ochsenbein); the following modifications were performed: => the positions were added from HD (=III/135) catalogue => there were initially 132 columns for lambda (the wavelength), 132 columns for the corresponding Fluxes and 132 columns for the mean errors. The lambda columns were removed; the corresponding fluxes and errors were moved to fixed positions. => unknown values, originally indicated by zero fluxes and " -" in the mean errors, have been blanked. II_86.xml Photographic Magnitudes for Stars at High Galactic Latitude 2087 II/87 Photographic Mags for Stars at High Galactic Lat Photographic Magnitudes for Stars at High Galactic Latitude D Weistrop CDS Bull. No. 24, p. 91 ??? ??? 1983 1983BICDS..24...91W Magnitudes, photographic Photometry, photographic Selected areas This is a catalogue contains photographically determined UBVr magnitudes for more than 13000 stars at high galactic latitude. Eight pieces of information are given for each star: identification number, approximate x and y coordinates as measured on the plates, V, B, U, r, and comments.
Data reg Region --- ID Star name --- X Approximate X coordinate on plate mm Y Approximate Y coordinate on plate mm V V magnitude mag B B magnitude mag U U magnitude mag r r magnitude mag rem Comments --- N.G. Roman ADC/SSDOO 1997 Nov 07 II_87.xml Four-Colour uvby and H-beta Photometry of A5 to G0 Stars Brighter than 8.3 mag 2090 II/90 Four-Colour uvby and H-Beta Phot A5-G0 Stars < 8.3 mag. Four-Colour uvby and H-beta Photometry of A5 to G0 Stars Brighter than 8.3 mag E H Olsen Astron. & Astrophys. Suppl. 54 55 1983 1983A&AS...54...55O Photometry, uvby Photometry, H-beta The catalog resulted from a photometric survey of HD stars of types A5 to G0 brighter than m(v) = 8.3. The author compiled the data set to provide a complete, magnitude limited, kinematically unbiased sample of late F-type stars belonging to the intermediate population II. The catalog consists of ten files. The first, catalog.dat, contains the main catalog data, compiled from eight smaller catalogs (one from each part of the observing program). Table13.dat through table19.dat contain lists of uvby standard stars transformed to the Crawford-Barnes system (Crawford and Barnes 1970). Table23.dat and table24.dat contain beta standard stars transformed to the Crawford-Mander system (Crawford and Mander 1966). The main catalog file lists for each of 14816 stars its identification, V magnitude and error, uvby indices and errors in the Crawford-Barnes standard system, beta and error in the Crawford-Mander standard system, weightings, number of observations, and difference between standard and transformed values for the standard stars used in reducing the observational data.
Main catalog data Ident HD, Durchmusterung, or AGK number, & component --- V V magnitudes in the Johnson UBV system mag e_V mean error on V The internal rms error of one observation computed as M.E. = sqrt[ (total residual)^2/(w -1)], where w is the number of observations, all observations having weight 1. See Olsen (1983) for a discussion of how this and all other errors were determined. mag b-y b-y index in the Crawford-Barnes system mag e_b-y Internal rms error in b-y mag m1 m1 index in the Crawford-Barnes system mag e_m1 Internal rms error in m1 mag c1 c1 index in the Crawford-Barnes system mag e_c1 Internal rms error in c1 mag w_V V magnitude weight V magnitude weight (a V measured on a cloudy night has a weight of 0) --- w_uvby uvby weight uvby weight includes b - y, m1, and c1 weight --- o_uvby uvby nights Number of nights of four-color (including V) observations --- beta beta in the Crawford-Mander system mag e_beta Internal rms error in beta mag w_beta beta weight --- o_beta Number of nights during which beta was observed --- rem Remark Single-character code. "*" indicates the presence of a note in the published version of the catalog (see Olsen 1983 for the text of these notes). The following letters are used to flag objects added to the original observing list for various reasons: C - Star used as a comparison star by the Copenhagen University Observatory group studying eclipsing binaries D - Double-line spectroscopic binary discovered by Andersen and Nordstrom (1977) "regularly observed in the hope of detecting eclipses" I - F and G-type supergiants monitored for long-term light variations N - Visual double star not listed in the Index Catalogue of Visual Double Stars (Jeffers et al., 1963) R - Metal-weak stars from other lists independently rediscovered during the uvby survey of the southern sky W - Five metal-weak stars from the Michigan Schmidt survey plus 45 stars from Bidelman and MacConnell's list brighter than m(v) = 8.5 --- uvby standard stars uvby standard stars uvby standard stars uvby standard stars uvby standard stars uvby standard stars uvby standard stars Ident HR number(s) --- V V magnitude transformed to the Johnson system mag e_V rms error of a single observation with weight 1 in magnitudes mag b-y b-y transformed to the Crawford-Barnes system mag e_b-y rms error in b-y for a single observation in magnitude mag m1 m1 transformed to the Crawford-Barnes system mag e_m1 rms error in m1 for a single observation in magnitude mag c1 c1 transformed to the Crawford-Barnes system mag e_c1 rms error in c1 for a single observation in magnitude mag w_V V magnitude weight --- w_uvby weighting of uvby indices --- o_uvby Number of obs. on which the star was observed --- V-diff The difference between standard and transformed V magnitude mag b-y-diff The difference between standard and transformed b-y magnitude mag m1-diff The difference between standard and transformed m1 magnitude mag c1-diff The difference between standard and transformed c1 magnitude mag beta standard stars beta standard stars Ident HR number --- beta beta magnitude mag e_beta mean error on beta error of a single observation with weight 1 in magnitudes mag w_beta beta weight --- o_beta Number of nights on which the star was observed --- diff The difference between standard and transformed beta in magnitudes mag M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1996 May 10 UNKNOWN UNKNOWN Four-colour uvby and H_Beta Photometry of A5 to GO stars brighter than m(v) = 8.3 (UVBYbeta) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in November 1983. The catalog consisted of ten files: one main data file and nine standard star lists. Eight bytes containing the file identification were deleted from the beginning of all records in every file, and blank columns were removed by means of an editor. As a result, the record sizes were reduced from 124, 132, and 52 bytes to 94, 96, and 30 bytes, respectively. II_90.xml The Stellar Component of the Galaxy as seen by the AFGL Infrared Sky Survey 2095 II/95 Stellar Component of the Galaxy, AFGL IR Survey The Stellar Component of the Galaxy as seen by the AFGL Infrared Sky Survey G L Grasdalen R D Gehrz J A Hackwell M Castelaz C Gullixson Astrophys. J. Suppl. 53 413 1983 1983ApJS...53..413G Photometry, infrared Surveys Measurements at 2.3, 3.6, 4.9, 8.7, 10, 11.4, 12.6, 19, and 23 microns are included in this catalog based on observations by the Wyoming Infrared Observatory. The sources included are those from the AFGL survey with the 4mu magnitude brighter than +1.3, the 11mu magnitude brighter than -1.5, or the 20mu magnitude brighter than -4, which lie between 20 and 40 minutes in each hour of right ascension.
Data AFGL AFGL number --- IRCzone IRC zone --- IRCnum IRC number within zone --- BS BS number = HR --- BDzone BD zone --- BDnum BD number within zone --- ID Other Identification --- varType Type of Variable Star --- Period Period of variation d Sp Spectral Type --- r_Sp Source of spectral type DO = Dearborn Catalog of Faint Red Stars IRC = Infrared Catalog GCVS = General Catalogue of Variable Stars VOGT = Vogt (1973) H&B = Hansen & Blanco (1975) LWD = Lockwood (1974) HR = Yale Catalog of Bright Stars CK1 = Cohen & Kuhi (1976) CK2 = Cohen & Kuhi (1977) GC = Albany General Catalog CASE = Case surveys for late-type stars WWSJ = Wisniewski et al. 1967 H&L = Harvey and Lada (1980) GHB = Gehrz, Hackwell & Briotta (1978) HBG = Herbig (1956) --- Lum Luminosity class 2 = Luminosity Class I and II 3 = Luminosity Class III 4 = Luminosity Class IV 5 = Luminosity Class V 6 = Luminosity Class c 7 = Luminosity Class g 8 = Luminosity Class d --- RAh RA hours (1950) h RAm RA minutes (1950) min RAs RA seconds (1950) s DE- Sign of declination --- DEd Dec degrees (1950) deg DEm Dec minutes (1950) arcmin DEs Dec seconds (1950) arcsec ref Source of position SAO = Smithsonian Astrophysical Obs. Star Catalog JYCE = Joyce et al. (1977) G&H = Gehrz & Hackwell (1976), including unpublished positions WIRO = Positions determined at the WIRO GCVS = General Catalogue of Variable Stars SVS = Catalog of Suspected Variable Stars IRC = Infrared Catalog LADA = Lada et al. (1981) GC = Albany General Catalog AGK3 = Catalog der Astronomischen Gesellschaft LKVR = Low et al. (1976) LKRL = Lebofsky et al. (1976) KLMN = Kleinmann et al. (1979) AFGL = position from AFGL catalog GLG = Grasdalen (1974) REID = Reid et al. (1980) SSJ = Simon, Simon & Joyce (1979) BHR = Baldwin, Harris & Ryle (1973) HGSB = Hackwell et al. (1978) HGG = Hackwell, Grasdalen & Gehrz (1982) LSKR = Lebofsky et al. (1978) --- rem Comments C = comment about source exists in Table 4 --- class Note on detection FMQ = Sources seen reliably only at 4microns LL = Sources seen reliably at 11, 20,or 27 microns LST = Sources rejected from the WIRO survey --- mag Visual magnitude mag r_mag Source of mag (if any) --- I'Mag IRC I' Magnitude mag kMag IRC k Magnitude mag mag4 AFGL mag at 4 microns mag mag11 AFGL mag at 11 microns mag mag20 AFGL mag at 20 microns mag mag27 AFGL mag at 27 microns mag obs_day Day of WIRO observations --- obs_mo Month of WIRO observations --- obs_yr Year of WIRO observations --- mag2.3 WIRO magnitude at 2.3 microns mag mag3.6 WIRO magnitude at 3.6 microns mag mag4.9 WIRO magnitude at 4.9 microns mag mag8.7 WIRO magnitude at 8.7 microns mag mag10 WIRO magnitude at 10 microns mag mag11.4 WIRO magnitude at 11.4 microns mag mag12.6 WIRO magnitude at 12.6 microns mag mag19 WIRO magnitude at 19 microns mag mag23 WIRO magnitude at 23 microns mag obs WIRO observer GG = Gary Grasdalen JAH = John Hackwell RDG = Robert D. Gehrz BTA = Dan Briotta G&H = Gehrz & Hackwell (1976, and additional unpublished data) --- Comments on individual sources GL GL number If GL is blank, then text is continued from previous record. --- text Comment on individual source --- Julie Anne Watko SSDOO/ADC 1996 May 01 II_95.xml A Catalogue of H-beta Photometry of Southern A5 to G0 Stars Brighter than 8.3 magnitudes 2100 II/100 H-beta Photometry of Southern A5-G0 Stars < 8.3 mag A Catalogue of H-beta Photometry of Southern A5 to G0 Stars Brighter than 8.3 magnitudes E H Olsen C L Perry Astron. and Astrophys. Suppl. 56 229 1984 1984A&AS...56..229O Photometry, H-beta The catalogue of H-beta photometry of southern A5 to GO stars brighter than m(v) = 8.3 (Olsen and Perry 1984) is a compilation of H-beta photometry of southern stars extending to the southern sky the work done by Perry and Johnston (1982) and Perry et al., (1982). The catalog lists identification and beta value with mean error, weighting, and number of observations for 2,699 Southern stars. A second file lists the same information for 42 standard stars, transformed to the Crawford-Mander standard system.
Main catalog data ID HD number --- comp Component or blend --- beta Beta magnitudes mag e_beta Mean error on beta When total weight > 1 this is "the internal rms error of one observation," otherwise this is the overall rms error, in magnitudes mag w_beta Total weighting (each observation = 1) --- o_beta Number of nights the object was observed --- Standard stars data HR HR number --- beta Beta magnitudes beta transformed to the Crawford-Mander system, in magnitudes mag e_beta Mean error on beta When total weight > 1 this is "the internal rms error of one observation," otherwise this is the overall rms error, in magnitudes mag w_beta Total weighting the object was observed --- o_beta Number of nights the object was observed --- diff The difference between standard and transformed beta mag C.-H. Joseph Lyu Hughes STX/NASA 1996 May 10 UNKNOWN UNKNOWN A Catalogue of H-beta Photometry of southern A5 to GO stars brighter than m(v) = 8.3 was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in January 1985. The catalog tape contained two text files: the first listed the main catalog data, and the second listed the standard star data. Eight bytes holding the file identification were deleted from the beginning of all records in both files, and blank columns were removed by means of an editor to reduce the record size from 48 and 56 bytes to 25 and 30 bytes, respectively. II_100.xml Photographic UBV Photometry for Stars in Open Clusters 2104 II/104 Photographic UBV Photometry, Open Clusters Photographic UBV Photometry for Stars in Open Clusters J -C Mermilliod CDS Bull. No. 27, p. 141 ??? ??? 1984 1984BICDS..27..141M Clusters, open Photometry, UBV This catalog is a compilation of previously published UBV photographic photometry of over 34000 stars in 127 open clusters. The author has adopted a uniform numbering system (as used in some other catalogs) and translated the identifications of all stars to this system. References to the photometric data and the individual numbering systems are also included. The catalog is in three files: the first file lists the catalog data, the second lists the full forms of the references cited by code number in the first, and the third contains a list of references to the numbering schemes for each cluster.
Catalog data flag Catalog flag Single-digit integer flag indicates the catalog in which the cluster is listed: 2 NGC 3 IC 5 Anonymous cluster. There is only one of these in this catalog, Melotte 66. The catalog/cluster number for this cluster is 52066. --- Cl_num Cluster number in the catalog --- starNum Star number in the cluster (translated to the standard system where necessary) --- Comp Component number identifying a component of a multiple system or blank --- V V magnitudes mag B-V B-V magnitudes mag U-B U-B magnitudes mag RefCode Reference The full forms of the references are listed in the next file. --- References to the catalog data RefCode Code number by which the reference is cited --- Ref Reference Full form of the reference. When bytes 1-5 are blank, this field is a continuation of the previous record. --- Cluster reference codes and sources flag Catalog flag Single-digit integer indicating the catalog in which the cluster is found: 2 NGC 3 IC 5 Anonymous cluster. There is only one of these in this catalog, Melotte 66. The catalog/cluster number for this cluster is 52066. --- Cat Catalog number of the cluster --- suffix any star in cluster placeholder "BBBB" --- Ref Reference Full form of the reference. When bytes 1-12 are blank, this field is a continuation of the previous record. --- N.P.M. Kuin and C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 07 UNKNOWN UNKNOWN The preliminary Catalogue of Photographic UBV Photometry of Stars in Open Clusters (UBVOC) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in July 1985. The original tape consisted of four text files: the first contained a description of the catalog files, the second contained the main data file, the third listed the references cited by code number in the data file, and the fourth listed references to the cluster numbering systems. The information in the descriptive file has been incorporated into this document. Blank columns were removed from the second file by means of an editor to reduce the record size from 40 to 32 bytes, and the header records in the remaining two files were deleted. A FORTRAN program was run to check the validity of each field according to its data type and value. In the catalog file, a typographical error was discovered in record 29437 of the catalog file and corrected by referring to the source reference. Three data fields in the same file were also found to contain only a decimal point (one V and two B-V). These decimal points were replaced by blanks. Finally, at the suggestion of J.-C. Mermilliod, the cluster designations in the numbering file were slightly reformatted. A "+" preceding each number and a "." separating the catalog number from the remainder of the designation were both deleted so that these number would follow the same format as the identifications in the data file. No other changes have been made to any of the files. The catalog's original ADC documentation was scanned and included in the ReadMe file. During verification 1 error was found in data file catalog.dat: Record 35298 had a bad decimal point <0> in column 'U-B'. According to the context and the data format (F6.2), the bad data point was changed from 0057 to 0.57. II_104.xml A Search for Ultraviolet-Excess Objects 2106 II/106 Search for Ultraviolet-Excess Objects A Search for Ultraviolet-Excess Objects T Noguchi H Maehara M Kondo Ann. Tokyo Astron. Obs. 2nd series 18 55 1980 1980AnTok..18...55N A Search for Ultraviolet-Excess Objects M Kondo T Noguchi H Maehara Ann. Tokyo Astron. Obs. 2nd series 20 130 1984 1984AnTok..20..130K Photometry, ultraviolet The catalog is a list of 1186 ultraviolet-excess objects found during two surveys with the Kiso Schmidt telescope of the Tokyo Astronomical Observatory. The UGR three-image method was used to detect the objects cataloged, which range in blue magnitude from about 10.0 to 18.5. The table contains equatorial positions to an accuracy of about 0.5 seconds of arc (equinox and equator B1950.0, epoch of observation), magnitudes (green of the "three-image [UGR] method"), color indices (as estimated from the enhancement of the U image relative to the G), object codes (white dwarf, QSO, diffuse object, etc.), and alternate designations (in addition to a KUV coordinate designation).
Catalog data KUV_RA KUV coordinate designation - RA KUV coordinate designation is composed of hours and minutes of right ascension, sign, and degrees and minutes of arc of declination. Note that this coordinate designation does not follow the standard IAU convention because the coordinates are rounded and not truncated. --- KUV_DE KUV coordinate designation - DE --- Comp Component identification --- KISO_a KISO area number Another designation consisting of a Kiso area number (see Kiso Information bulletin No. 1, 1979) and a serial number within the area. --- KISO-n Number within KISO area --- RAh Right Ascension (hours), equinox 1950 h RAm RA (minutes) min RAs RA (seconds) s DE- sign of declination zone, equinox 1950 --- DEd DEC (degrees) deg DEm DEC (minutes) arcmin DEs DEC (seconds) arcsec G G magnitude The G (green) magnitude of the "three-image (UGR) method" used for efficient detection of blue objects, e.g., by Haro & Herbig (1955), Iriarte & Chavira (1957), Haro & Luyten *(1962), and others. See the source reference for additional details. A colon (:) in byte 54 denotes an uncertain value. mag u_G G uncertainty code --- CI Color index Estimated as the enhancement in the U image relative to the G, calibrated with known values of U-B color. A colon (:) in byte 59 denotes an uncertain value. mag u_CI CI uncertainty code --- Ocode Object code A letter object code to denote the following characteristics: W spectroscopically confirmed white dwarf Q quasar D diffuse object with possible accompanying halo V variable that is definitely brighter or fainter on print of the Palomar Observatory Sky Survey than on the Kiso plate --- Ref Alternate designation An alternate object designation in a previous catalog, composed of a reference number in bytes 63-64, followed by the designation in the cited catalog. --- M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1995 May 25 UNKNOWN UNKNOWN A magnetic tape containing the first and second Kiso Surveys in separate files was received from Dr. M. Kondo on March 11, 1985. The following modifications were made to produce the current catalog: 1. The two lists were moved to online storage and merged 2. Minus signs on negative declinations were moved to always occur in the same byte. Zero declinations had lost their signs; these were added by using the respective KUV designations. Plus signs were then added to all positive declinations. 3. Uncertainty codes for G magnitude were moved to byte 54 so that they do not occur within the magnitude field. 4. The combined list was sorted by increasing right ascension. II_106.xml The Two-Micron Sky Survey: Nearest SAO Star and Locations on Palomar Sky Survey Prints 2108 II/108 Two-Micron Sky Survey, Nearest SAO Stars on POSS The Two-Micron Sky Survey: Nearest SAO Star and Locations on Palomar Sky Survey Prints T A Nagy R S Hill J M Mead ADC Bull. 1 183 1983 1983 Surveys This catalog is a list of potential guide stars developed for a program to obtain more precise positions of objects in the IRC Two-Micron Sky Survey of Neguebauer and Leighton (1969). For each IRC source (col. 1), it gives: (col. 2) the identification of the star in the SAO catalog which is nearest, (col. 3) the great circle arc distance (in seconds) between the SAO star and the IRC source, (col. 4) the position angle (in degrees) of the IRC source relative to the SAO star, (col. 5) the plate number(s) of the POSS on which the IRC source appears, (col. 6,7) the approximate rectangular coordinates (in mm) of the IRC source on the POSS print area with respect to the Southwest corner, and (col. 8) the modified Luyten Palomar number. The POSS plate numbers given are for the red plates.
Catalog Data ID IRC Number from Two-Micron Sky Survey --- SAO ID of Closest SAO Star to IRC Source This datum is from the MATCH output data file. --- D Great Circle Arc Distance between SAO and IRC The published positions from the individual source catalogues are the data inputs to the MATCH program. Proper motion effects are not incorporated into the MATCH program. arcsec PA Position Angle of IRC Relative to SAO Source The angle is measured from North through East according to the standard convention. This quantity was computed from the published Epoch 1950.0 source positions. deg POSS POSS Plate ID The POSS plate ID for the plate area on which the IRC object appears. The plate IDs include the Palomar (Arabic numeral preceded by the letter S) and Whiteoak (IDs from 7000-9999) Southern Extensions. If an object appears on more than one POSS print area, a multiple listing is given for each print area on which the given object appears. The POSS Designations in this table are for the red plates. There are four different blue and red numbers as given below: POSS-E POSS-O MLP 9 10 465 14 15 469 15 16 472 11 12 473 --- X Rectangular Coordinate on POSS Print Area The values are measured with respect to the Southwest corner of the print area. The center of the print area is: X = 172.5 Y = 173.5 mm Y Rectangular Coordinate on POSS Print Area mm MLP Modified Luyten Palomar Number This number represents a sequential numbering of the POSS plus Whiteoak plate areas (range 1-1037). The overall sequence is from North to South; within each declination band it is by increasing Right Ascension. Therefore, plate 1 is at the North Pole and plate 1037 is at the Southern limit of the Whiteoak extension. This numbering scheme also takes into account the nearly duplicate POSS plate areas (895 and 1619) which correspond to MLP numbers 723 and 724 respectively. Since the two plate centers are almost identical, when a source is assigned to one of the plates, typically it is assigned to both. -------------------------------------------------------------------------------- --- Julie Anne Watko SSDOO/ADC 1995 Nov 03 II_108.xml A search for faint blue stars in high galactic latitudes. III. Twelve PSS fields at declinations -6{deg} and -12{deg} near the South Galactic Pole. 2111 II/111 Faint Blue Stars in high Galactic Latitudes III A search for faint blue stars in high galactic latitudes. III. Twelve PSS fields at declinations -6{deg} and -12{deg} near the South Galactic Pole. J Berger A M Fringant Astron. Astrophys. Suppl. Ser. 58 565 1984 1984A&AS...58..565B III/64 : Catalog of blue objects at high galactic latitude (Berger+ 1980) I. Berger J. & Fringant A.-M. 1977A&AS...28..123B II. Berger J. & Fringant A.-M. 1980A&AS...39...39B III. Berger J. & Fringant A.-M. 1984A&AS...58..565B IV. Berger J. & Fringant A.-M. 1985A&AS...61..191B Stars, blue Stars, faint Stars, faint blue QSOs stars: faint blue stars: early-type subdwarfs white dwarfs quasars: general galaxies: compact This is the third and last part of the survey of faint blue objects: a catalogue of 2484 starlike or compact objects is presented with the 1950 positions, estimated magnitudes, color classes and extensive identifications with stars of previous surveys and known QSO's.
The PB Catalog PB Serial number --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Bmag Estimated B magnitude (step of 0.5mag) mag Uclass Colour class from I (UV-richest objects) to III (described in Paper I) --- Note Flag for an existing note (file notes) --- Remark Remarks about identification with previously known objects, and/or nature of the non-stellar like object number=1 the nature of the object is GALAXY, or CP.OBJ. (compact object), or M.CP.OBJ. (moderately compact object). --- Notes to PB objects PB Serial number --- Cont Continuation letter --- Text Text of note. number=1 colour classes are designated by lowercase b, a, f, g, k, or m ; the acronyms used for designations of the objects are: F = Feige (1958ApJ...128..267F) G = Giclas et al., "The G numbered stars" (cat. <I/79>) GD = Giclas et al., 1980, Lowell Obs. Bull. 8, 157 K = Noguchi et al. (1980AnTok..15...55N) LB = Luyten & Miller, 1956, "A search for faint blue stars", Univ. Minnesota, Minneapolis LP = Louten & La Bonte, 1973, "The South Galactic Pole" MCG = Morphological Catalog of Galaxies, Cat. <VII/62> and <VII/100> NLTT = Luyten, 1979, Cat. <I/98> PHL = Haro & Luyten, 1962BITon...3...37H, Cat. <III/74> --- Francois Ochsenbein CDS 1997 Aug 04 II_111.xml A Catalog of Ultraviolet Interstellar Extinction Excesses for 1415 Stars 2114 II/114 UV Interstellar Extinction Excesses for 1415 Stars A Catalog of Ultraviolet Interstellar Extinction Excesses for 1415 Stars B D Savage D Massa M R Meade P R Wesselius Astrophys. J. Suppl. 59 397 1985 1985ApJS...59..397S Interstellar medium This catalog contains ultraviolet interstellar extinction excesses in the ultraviolet region, as derived from five-channel Astronomical Netherlands Satellite (ANS) UV photometry. The rectangular bandpasses had central wavelengths of 1549, 1799, 2200, 2493, and 3294 angstroms with widths of 149, 149, 200, 150, and 101 angstroms, respectively. Color excesses were derived for each UV BD wavelength with reference to the V filter of the UBV system as well as a measure of excess extinction in the 2200-angstrom bump. The photometric data used were taken from the ANS Ultraviolet Photometry Catalogue of Point Sources (Wesselius et al. 1982), and excesses were derived for 1415 stars with spectral types of B7 and earlier. Data in the catalog include: object identification in a uniform format; right ascension and declination (1950); galactic coordinates estimated distance based on MK type; V magnitude and spectral type taken from the ANS catalog; color excesses E(B-V), E(33-V), E(25-V), E(22-V), E(18-V), E(15-V); extinction parameter E(Bump); Delta parameters for the bump: and (15-V) (measuring the deviation of the extinction curve affecting a given star from the sample mean curve, normalized by the rms scatter of the entire sample), and comment codes for variability, cluster proximity, and duplicity. The UV extinction measures are appended by uncertainty flags where appropriate. Other data include identification of stars exhibiting peculiar UV extinction, and basic positional, photoelectric and spectral-type information.
catalog data Ident Object identification Object identification- includes catalog name and number in The Henry Draper Catalogue (Cannon and Pickering 1918-1924; Cannon 1925-1936; Cannon and Walton Mayall 1949), in one of the Durchmusterung catalogs, or in the catalog of Feige (1958, 1959). The catalog identification is always in bytes 1-3 and the number in bytes 4-12, and the field is entirely homogeneous so that the complete catalog can be sorted by object ID. --- RAh Right ascension, equinox 1950. h RAm R.A. (minutes) min RAs R.A. (sec) s DE- Sign of declination, equinox 1950. --- DEd Dec. (degrees) deg DEm Dec. (minutes) arcmin GLON Galactic longitude, l. deg GLAT galactic latitude, b deg dist Distance estimate based on Blaauw's (1963) M(V) - spectral-type calibra- tion and A(V) = 3.1E(B-V). pc V V magnitude taken from ANS catalog. mag Sp Spectral type / luminosity Spectral type taken from the ANS catalog, wherein the original sources are: Jaschek (1978), Houk and Cowley (1975), Houk (1978), Buscombe (1977,1980), other sources, in the priority given; or from the HD. The format is uniform with temperature classes in byte 56, sub-classes in 57-59, and luminosity classes/peculiarities in 60-65. Several incorrect spectral types in the ANS catalog have been corrected here. Whereas the luminosities and peculiarities are all in upper case in the published catalog, they have been converted to upper/lower case in this machine version according to standard notation. --- E(B-V) Color excess E(B-V). mag E(33-V) Color excess E(33-V). mag flag1 Extinction parameter flag Extinction parameter flag for E(33-V). A colon (:) indicates a parameter derived from ANS data with 1 standard deviation statistical errors between 5% and 15%. This applies to the colon flags on all color excesses following [but not to E(Bump)]. --- E(25-V) Color excess E(25-V). mag flag2 Flag for E(25-V). --- E(22-V) Color excess E(22-V). mag flag3 Flag for E(22-V). --- E(18-V) Color excess E(18-V). mag flag4 Flag for E(18-V). --- E(15-V) Color excess E(15-V). mag flag5 Flag for E(15-V). --- E(Bump) Extinction parameter E(Bump) Extinction parameter E(Bump), the excess extinction in the bump measured with respect to a linear (g-1) "background" extinction defined by the ANS photometric bands at 1800 and 2500 A: E(Bump) = E(22-V) - 0.35E(18-V) - 0.65E(25-V). mag flag6 Extinction parameter flag for E(Bump), present if its photometric error is >5%. In the extreme case, a cataloged value of E(Bump) can contain a cumulative photometric error of 19%. --- Del(Bump) ?=-9.99 Magnitude difference Delta(Bump) Magnitude difference Del(Bump) represents the deviation of the extinction curve affecting a given star from the sample mean curve, normalized by the rms scatter of the entire sample. Magnitude difference (diff) values are not given for stars having E(B-V) <= 0.1 mag, since parameters derived from stars having small color excesses are much too unreliable. The default is -9.99. mag flag7 Magnitude difference Delta(Bump) parameter flag A colon indicates that an E(x) with photometric uncertainty >5% entered the calculation of magnitude difference (x). --- Del(15-V) =-9.99 Magnitude difference Delta(15-V) See the note on Delta(Bump) mag flag8 Magnitude difference Delta(15-V) parameter flag (See byte 121.) --- code Comment character codes Character codes denote the following: C : cluster star in crowded field, with possible UV data contamination; D : star is listed in a source other than the Strasbourg Catalog of Stellar Identifications (CSI; Ochsenbein, Bischoff and Egret 1981) as double. E?: possible anomalous extinction (reddening) law; V : the UV results indicate variability; V?: suspected variable (for some of these objects, the ground-based information might be erroneously listed in the source catalogs); --- N.P.M. Kuin and C.-H. Joseph Lyu Hughes STX/SSDOO/NASA 1995 Jun 09 UNKNOWN UNKNOWN A magnetic tape containing A Catalog of Interstellar Extinction Excesses for for 1415 Stars was kindly supplied by the authors on 24 June 1985, along with a preprint of the published paper and a physical tape description. The entire catalog was transferred to disk storage and compared against the printed catalog. The following modifications were made: 1. The object identifications were homogenized and the catalog codes (HD, BD, CD, FEI) added. These are now entirely uniform and all numbers are right justified so that the whole catalog can be sorted by object ID if desired. 2. Signs were added to positive values of Dec. deg; minus signs were removed from Dec. '; minus signs were missing from declinations in the -00 deg zone. These stars were all looked up (+00 deg and -00 deg) in other catalogs and appropriate signs added. (This error does not occur in the published catalog.) 3. Signs were also added to positive values of galactic latitude, to magnitude difference (Bump) and to magnitude difference (15-V). June 1995: The catalog documentation was converted to standard form. Blanks in the galactic lattitude field were converted to zero's to have valid values with the sign included rather than a separate field for the sign. II_114.xml Faint Blue Objects at High Galactic Latitude. Catalog of Objects in SA28, 29, 55, 57 and 94 2115 II/115 Faint Blue Objects at High Galactic Latitude Faint Blue Objects at High Galactic Latitude. Catalog of Objects in SA28, 29, 55, 57 and 94 A Warnock III P D Usher ADC Bull. 1 195 1982 1982 Blue objects Stars, blue Stars, faint Stars, faint blue The data set of Faint Blue Objects at High Galactic Latitude is a catalog of objects selected according to relative ultraviolet excess from ubv three-color 1.2-m Palomar Schmidt plates. Five selected area fields centered on SA28, SA29, SA55, SA57 and SA94 are included. The data consist of color classifications, B magnitudes, 1950 equatorial coordinates and remarks; the current file contains 3678 objects. Three selected area fields were included originally, centered on SA57 (Usher 1981), SA29 (Usher, Mattson and Warnock 1982) and SA28 (Usher and Mitchell 1982). Areas centered on SA55 and SA94 were added in 1984.
Catalog data SeqNum US (sequential number; SA57 (1-634), SA29 (635-1184), SA28 (1185-2363), SA55 (2364- 3101), SA94 (3102-3678). --- Color Color class Color class is based on the following criteria: For U-V < 0: 1A - Above the blackbody (BB) line by delta(U-B) >= 0.15 mag; region populated mainly by quasars. 1 - Within delta(U-B) approx. +/- 0.15 mag of BB line. 1B - Below BB line by delta(U-B) approx. 0.15 mag (in general vicinity of white dwarf cooling curve). 1BS - Close to the luminosity class III-V line for blue halo stars. For U-V >= 0: 1C - Above the BB line in the region where type N and continuous spectrum galaxies often located. 2 - Below the BB line, but not within the color class 3 region. 3 - Within the region of the subdwarfs and halo horizontal-branch stars. The class field can contain a colon (:) indicating uncertainty, an exclamation point (!) or a question mark (?). --- B B magnitude was determined by iris photometry mag flag Colon (:) for uncertain magnitude --- RAh Right ascension for equinox 1950 (hours) h RAm R.A. (minutes) min RAs R.A. (seconds) s DE- Sign of declination. --- DEd Dec. for equinox 1950 (degrees) deg DEm Dec. (arcminutes) arcmin DEs Dec. (arcseconds) arcsec Rem1 Notes from original catalogs In the notes from original catalogs, the following abbreviations are employed: E: edge zone -- object within approx. 1 deg of plate edge G: galaxy, as determined from morphology plate CG: compact galaxy C: confused source Q: known quasar (from Veron and Veron 1974 and succeeding papers) ?: uncertainty R: remark in bytes 59 to 118 --- fieldID Field identification (SA57, SA29, SA28). --- Rem2 Additional remarks. --- M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1995 May 25 UNKNOWN UNKNOWN The Faint Blue Objects at High Galactic Latitude data file was received on magnetic tape from A. Warnock III on 2 April 1982. The only modifications made to the file were that the B magnitude field was converted to a blank field when no value is given (it was 0.0 when received) and the logical record length was changed from 132 bytes to 118 bytes, since bytes 119 to 132 were never used. Additional data for SA55 and SA94 were received in 1984 and were incorporated into the existing catalog in the same format. For a discussion of the methods employed in object selection, see Usher (1981) and Warnock and Usher (1982). II_115.xml Photoelectric Photometric Catalogue in the Johnson UBVRI System 2116 II/116 Photoelectric Photometry in Johnson UBVRI System Photoelectric Photometric Catalogue in the Johnson UBVRI System T Lanz Astron. Astrophys. Suppl. Ser. 65 195 1986 1986A&AS...65..195L II/7A : UBVRIJKLMNH Photoelectric Catalogue (Morel and Magnenat 1978) Kunkel, W.E., and Rydgren, A.E. =1979AJ.....84..633K Mermilliod, J.-C. 1978, Bull. Inform. CDS 14, 32 =1978BICDS..14...32M Moffett, T.J., and Barnes III, T.G. =1979PASP...91..180M Morel, M., and Magnenat, P. 1978, A&AS, 34, 477 =1978A&AS...34..477M (CDS Catalogue: II/7A) Neckel, T., and Chini, R. =1980A&AS...39..411N Photometry, UBVRI The catalog is a compilation of photoelectric photometry in the Johnson UBVRI system published prior to mid-1984. The catalog contains a total of 6849 stars in the original Johnson system (Morel and Magnenat 1978), 467 stars in the system of Kunkel and Rydgren (1979), 1150 stars in the system of Moffett and Barnes III (1979), and 252 stars in the system of Neckel and Chini (1980). The catalog is in 14 files: The first 12 files list observational data, mean values, and references for each of the four standard systems. An additional two files contain the numbering scheme of Mermilliod (1978) used to identify objects, and introductory information.
Homogenized photometry in Johnson UBVRI system Homogenized photometry in Kunkel+Rydgren system Homogenized photometry in Moffett+Barnes system Homogenized photometry in Neckel+Chini system LID Object identification in Lausanne/Geneva system (see file "codes.txt") --- m_LID 'D' for unresolved binary, or component number --- VarFlag 'V' if star is variable --- Vmag V magnitude in the Johnson UBVRI system mag U-B U-B color in the Johnson UBVRI system mag B-V B-V color in the Johnson UBVRI system mag V-R V-R color in the Johnson UBVRI system mag R-I R-I color in the Johnson UBVRI system mag Imag I magnitude in the Johnson UBVRI system mag Weight Weight of the photoelectric data, derived from number of measurements --- Observations in Johnson UBVRI system Observations in Kunkel+Rydgren system Observations in Moffett+Barnes system Observations in Neckel+Chini system LID Object identification in Lausanne/Geneva system (see file "codes.txt") --- m_LID 'D' for unresolved binary, or component number --- VarFlag 'V' if star is variable --- Vmag V magnitude in the Johnson UBVRI system mag U-B U-B color in the Johnson UBVRI system mag B-V B-V color in the Johnson UBVRI system mag V-R V-R color in the Johnson UBVRI system mag R-I R-I color in the Johnson UBVRI system mag Imag I magnitude in the Johnson UBVRI system mag n_NumObs Qualifying code for NumObs number=1 the code takes the following values: '/' the actual number of observations was not listed in the source reference; '1' was assumed '*' there were at least as many observations as given by value of NumObs 'S' standard star; exact number of observations not known --- NumObs Number of observations --- Ref Reference Number(file "refs.dat") --- Explanations of References Ref Reference Number, blank for continuation lines number=1 The numbers are: 08001 to 08115 for Johnson UBVRI system 68001 to 68014 for Kunkel and Rydgren system 72001 to 72011 for Moffett and Barnes system 73001 to 73007 for Neckel and Chini system --- Text Text of bibliographical reference --- adc.doc ASCII original documentation made at ADC adc.tex LaTeX documentation made at ADC codes.txt Explanation of the LID designations Francois Ochsenbein CDS 1995 Oct 20 UNKNOWN UNKNOWN * See section 3 of the document file "adc.doc" of "adc.tex" (Anne C. Raugh, 1987) * On the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1991), directory /photom/lanz * 20-Oct-1995: merged all references files into a single one at CDS. II_116.xml A Catalog of Concentric Aperture UBVRI Photoelectric Photometry of Globular Clusters 2117 II/117 Catalog of UBVRI Photometry of Globular Clusters A Catalog of Concentric Aperture UBVRI Photoelectric Photometry of Globular Clusters C J Peterson PASP 98 192 1986 1986PASP...98..192P Photometry, UBVRI Photometric data directly obtained in UBVRI or converted to UBVRI magnitudes are tabulated. The data comprise approximately 4600 records from 56 individuals and contains data unpublished at the time of the compilation as well as published data.
This catalog of globular cluster magnitudes includes both measurements originally obtained on that system and those obtained in other systems which have been converted to the UBVRI system. The equations used for this conversion are given in the source reference. No attempt has been made to put all observations on the same system otherwise. Although both northern and southern UBV data match the original Johnson system, the R and I photometry may differ due to differences in photocells and filters used in defining various sets of standard stars.
Data name Cluster Name --- code Reference Code Literature reference for data entry, following the code of refs.dat --- ap Aperture Diameter arcmin U U Magnitude Computed from V+(B-V)+(U-B) if all data exist for given aperture; otherwise the column is left blank mag U-B Johnson Ultraviolet Color Index mag B B Magnitude Computed from V+(B-V) mag B-V Johnson Blue Color Index mag V V Magnitude mag V-R Visual-Red Color Index mag R R Magnitude Computed from V-(V-R) mag V-I Visual-I Band Color Index Generally computed from (V-R)+(R-I) in the original sources of data mag I I Magnitude Computed from V-(V-I) mag References code Reference Code --- ref Reference --- N Number of Clusters --- type Type of Data --- Julie Anne Watko SSDOO/ADC 1996 Feb 21 II_117.xml UBVRI Photometric Standard Stars Around the Celestial Equator 2118 II/118 UBVRI Photometric Standard Stars, Celestial Equator UBVRI Photometric Standard Stars Around the Celestial Equator A U Landolt AJ 88 439 1983 1983AJ.....88..439L Photometry, UBVRI Stars, standard Stars, equatorial The catalog contains UBVRI photoelectric observations of 223 stars, mostly in an approximately 2-degree zone centered on the celestial equator. The catalog is intended to provide a uniform set of new standards, available to various sizes of telescopes in both hemispheres, on an internally consistent, homogeneous system. Most of the stars are in Selected Areas 92-115 and fall in the magnitude range of about 7 to 12.5 in V and color range -0.3 to +2.0 in B-V. The data include equatorial coordinates, photoelectric magnitudes and colors, numbers of observations, and computed internal errors.
Catalog Data cat Catalog abbreviation --- ID Number in catalog --- supp BD supplement letter (Barnard star) --- RAh Right ascension hours (1985.0) Positions are for equinox 1985 at epoch. However, proper motions have been accounted for in computing the 1985 coordinates for the large proper-motion stars, so these positions are given for equinox and epoch 1985.0. h RAm Right ascension minutes (1985.0) Positions are for equinox 1985 at epoch. However, proper motions have been accounted for in computing the 1985 coordinates for the large proper-motion stars, so these positions are given for equinox and epoch 1985.0. min RAs Right ascension seconds (1985.0) Positions are for equinox 1985 at epoch. However, proper motions have been accounted for in computing the 1985 coordinates for the large proper-motion stars, so these positions are given for equinox and epoch 1985.0. s DE- Sign of declination --- DEd Declination degrees (1985.0) deg DEm Declination degrees (1985.0) arcmin DEs Declination degrees (1985.0) arcsec V V magnitude Weighted V magnitude on the UBVRI photometric system, as defined by stars in Landolt (1973) and Cousins (1976). The colors are similar weighted means. mag B-V B-V color mag U-B U-B color mag V-R V-R color mag R-I R-I color mag V-I V-I color mag o_V Number of observations in weighted means --- no_V Number of nights on which star was observed --- e_V Mean error of V The mean error of a single observation of V or a color can be found by multiplying the appropriate error of the mean by the square root of n. mag e_B-V Mean error of B-V mag e_U-B Mean error of U-B mag e_V-R Mean error of V-R mag e_R-I Mean error of R-I mag e_V-I Mean error of V-I mag n_V Note flag(s) Number(s) referring to notes given at the top of the remarks file. These notes are distinct from the additional information given in Appendix I, which follows the "Notes" section in notes.txt. --- doc.txt ASCII version of ADC doc. (more detailed) doc.tex LaTeX version of ADC document notes.txt Remarks N. G. Roman SSDOO/ADC 1997 May 27 Warren expressed appreciation to A. U. Landolt for providing the catalog on magnetic tape and for reviewing and commenting on a preliminary version of this document prior to its finalization for distribution with the machine-readable catalog. This document has been derived from doc.txt. UNKNOWN UNKNOWN The machine-readable data table UBVRI Photometric Standards Around the Celestial Equator was received on magnetic tape from Dr. Arlo U. Landolt on 15 April 1986. Various modifications were made by Wayne. H. Warren at the ADC in order to effect a uniformly formatted data file, to isolate the table notes from the data, and to add the additional information contained in Appendix I of the published paper. II_118.xml Stellar Distribution Near the South Galactic Pole, Photographic V Magnitudes and (B-V) Colours of 640 Stars in Region I 2119 II/119 Stellar Distribution near the South Galactic Pole Stellar Distribution Near the South Galactic Pole, Photographic V Magnitudes and (B-V) Colours of 640 Stars in Region I B J Bok J Basinski Mem. Mount Stromlo Observatory No. 16, ??? ??? 1964 1964MmMtS..16.....B Colors Galactic pole, south Magnitudes, photographic This catalog contains a field of 2.8 square degrees centered on Kapteyn Selected Area 141 (l=245, b=-86). The center of field was near SAO 166815 (Bok I 174 B) at 01h05m11s -29d33'12"(1950). The covered ranges were 01h01m30s< RA < 01h09m30h and -30d20' < Dec < -28d35'(1950). Photographic V magnitudes and B-V colors of 640 stars were measured in Region I. Data were card punched at the Australian National University on an Univac 1100/82. The coordinates were determined by Kavan U. Ratnatunga from PDS scans of the region on UKSTU Schmidt plate J6657S (taken on 03-Jan-1981) and visual cross identifications were given with the published finding chart. The coordinate calibration used the positions of SAO stars. Estimated rms accuracies for the following measurements are: Visual Magnitude: 0.03 mag B-V colors : 0.05 mag Positions : 1 arc second
The catalogue Num Sequential number --- Ident Star identification --- Flag "B" for stars with V < 14.50, "F" for those with V >= 14.50. --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec Pmag Photographic V magnitude. mag B-V Photographic B-V color --- N.P.M. Kuin, C.-H. Joseph Lyu NASA Joseph Florsch CDS 1995 Jun 09 UNKNOWN UNKNOWN Data format modified at the Astronomical Data Center (ADC)/NASA GSFC, 1988 March...WHW Data description (prepared at the ADC/NASA GSFC, 1988 March...WHW) Converted to standard format: Intro file by Joseph Florsch (CDS) updated ReadMe by C.-H. Joseph Lyu (Huhges STX); corrections in position values from 60 seconds to +1 minute by Paul Kuin (ADC). II_119.xml A Photometric and Spectrophotometric Investigation in a Region at the South Galactic Pole 2120 II/120 Phot and Spectrophot Investigation, South Gal Pole A Photometric and Spectrophotometric Investigation in a Region at the South Galactic Pole P -I W Eriksson Uppsala Astron. Obs. Report 11 ??? ??? 1978 1978 Galactic pole, south Photometry, UBV Spectrophotometry Photoelectric magnitudes and colors in the Johnson-Morgan UBV system for 477 stars in 6 square degrees near Kapteyn Selected Area 141 (l=245, b=-86; 00 43 < RA < 01 11, -33.7 < Dec < -26.9, B1950.0) are given in the first data file. The estimated rms accuracies are 0.02 (V), 0.03 (B-V), 0.07 (U-B) for stars in the magnitude range 15 to 16. Table 2 of the source reference gives the mean errors for intervals of magnitude. Photographic V magnitudes and B-V colors are given for 2835 stars to magnitude 17 (in the same region as above) in the second data file. The estimated rms accuracies are 0.05 (V) and 0.08 (B-V). The mean errors of the computed right ascensions and declinations are 0.15s and 2", respectively.
Photoelectric data SeqNumb Sequential number --- ID Star number in the Henry Draper (HD) Catalogue or the Cordoba Dirchmusterung (CD) --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- Declination sign --- DEd Declination (degrees) (B1950) deg DEm Declination (minutes) arcmin V Photoelectric V magnitude. mag B-V Photoelectric B-V color mag U-B Photoelectic U-B color (value missing for SeqNumb = 215) mag Photographic data ID Star number in declination zones of 10', in the form XX.Y.zzzz: XX=degrees of southern declination. Y=tens digit of minutes of arc zzz=current number in the zone In the form XX.Y.zzzz: XX=degrees of southern declination. Y=tens digit of minutes of arc zzz=current number in the zone --- RAh right ascension B1950 (hours) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination B1950 (degrees) deg DEm declination (minutes) arcmin V Photographic V magnitude V and B-V are missing for star 30.2.204 -- the fields are blank. mag B-V Photographic B-V color mag N.P.M. Kuin, C.-H. Joseph Lyu NASA Joseph Florsch CDS 1995 Jun 09 UNKNOWN UNKNOWN The data were keypunched for Kavan U. Ratnatunga in 1982 June at the data center of the Australian National University, Canberra. They were supplied to the Astronomical Data Center/NASA Goddard Space Flight Center by K. Ratnatunga in 1986 April. Data format modified at the Astronomical Data Center (ADC)/NASA GSFC, 1991 October...Wayne H. Warren Jr. Errors corrected at CDS consecutive signs +- in Table pe, col. U-B, line 215 (missing value) Table pg, col. B-V, line 805 (29.3.096) (two consecutive signs +-) Table pg, col. B-V, line 2637 (30.5.048) (two consecutive signs +-) Changes made at ADC: pe.dat: changed in record 155, 268, 335 positions in RA with RAs=60 to RAm=RAm+1 and RAs=00. II_120.xml Stellar Distribution Near the Selected Areas 127, 141 and 189 2121 II/121 Stellar Distribution Near SA 127, SA 141, SA 189 Stellar Distribution Near the Selected Areas 127, 141 and 189 K U Ratnatunga Ph.D. Dissertation, The Australian National University, Canberra ??? ??? 1983 1993 Selected areas Stellar distribution Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.
SA 127 field SA 141 field SA 189 field RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) In numerous records the seconds are equal to 60 s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec J Photographic J magnitude = V + 0.841*(B-V) mag F Photographic F magnitude = V - 0.605*(B-V) mag C.-H. Lyu Hughes STX/NASA and Francois Ochsenbein CDS 1995 May 25 UNKNOWN UNKNOWN Data format modified at the Astronomical Data Center (ADC)/NASA GSFC, 1991 October...Wayne H. Warren Jr. Data description (prepared at the ADC/NASA GSFC from separate descriptions supplied by K. U. Ratnatunga, with format description added, 1991 November...WHW). UNKNOWN UNKNOWN Remarks on Plate Information: ----------------------------------------------------------------------------- J = IIIa-J KODAK emulsion + 2mm GG395 Schott glass filter = V + 0.841*(B-V) F = IIIa-F KODAK emulsion + 3mm RG630 Schott glass filter = V - 0.605*(B-V) ----------------------------------------------------------------------------- ---------------------------------------------------------------------------- SA Plate Observation Air Exposure Min Image Sky Back Limiting Number Date Mass Diameter Bright Density Magnitude (min) (microns) (mag) (mag) ---------------------------------------------------------------------------- 127 J7438S 05-JAN-1982 1.05 15 60 20.5 1.27 19.5 127 R7407S 20-DEC-1981 1.22 30 85 20.0 0.90 17.7 141 J7168S 03-JAN-1981 1.00 15 50 21.2 0.44 19.5 141 R6856S 14-NOV-1980 1.17 12 60 21.3 0.40 17.4 189 J7227S 30-SEP-1981 1.14 15 35 21.3 0.34 19.5 189 R7215S 22-SEP-1981 1.16 30 50 20.2 0.74 18.2 ---------------------------------------------------------------------------- Remarks on Field Information: ------------------------------------------------------------ SA l b Field RA (1950) Dec No. stars d d (sq.deg) h m h m d d ------------------------------------------------------------ 127 272 +38 20.9 11 00 to 11 20 -20 to -16 35786 141 245 -86 22.5 01 00 to 01 20 -32 to -37 13612 189 277 -50 20.9 02 50 to 03 30 -62 to -58 31088 ------------------------------------------------------------ Coordinate calibration used positions of SAO stars. Estimated rms accuracy for Best Magnitude range 13.5 < V < 16.0: Visual magnitude 0.05 mag (B-V) color 0.07 mag Positions 1 second of arc *** magnitudes brighter than 12 and fainter than 17.5 inaccurate *** II_121.xml UBV Photoelectric Photometry Catalogue (1986): I. The Original data 2122B II/122B UBV Photoelectric Catalog: data 1953-1985 UBV Photoelectric Photometry Catalogue (1986): I. The Original data J -C Mermilliod Astron. Astrophys. Suppl. Ser. 71 413 1987 1987A&AS...71..413M II/193 : Catalogue (1986-1992 Data) Jennens, P.A., and Helfer, H.L., 1975, MNRAS 172, 667. Johnson, H.L., and Morgan, W.W., 1953, ApJ 117, 313. Kunkel, W.E., and Rydgren, A.E., 1979, AJ 84, 633. Lanz, T., 1986, A&AS 65, 195. Moffett, T.J., and Barnes, T.G., 1979, AJ 84, 627. Neckel, Th., and Chini, R., 1980, A&AS 39, 411. Nicolet, B., 1975, A&AS 22, 329 Photometry, UBV The catalogue collects all UBV photoelectric photometry data published since 1953 to the end of 1985 in the Johnson and Morgan system. In addition, data obtained in closely related systems using UBV filters have also been collected. All the data have been merged, yielding a final catalogue of 136719(*) entries concerning 87267 stars and components. The data have been taken from 1413 (UBV) and 127 (other) references found in 73 different periodicals. Great care has been taken to detect and correct all kinds of errors. (*) Two entries have been deleted in version 'B' of this catalogue The analysis of the data is published in A&AS 71, 119 (1987)
Measurements in Johnson UBV system *Measurements in closely related UBV filters Merged data from ubv and ubva LID Code number (see file codes.txt) number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. --- Rem Remark on duplicity or identification of components the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. --- Var Remark on variability The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. --- Vmag V magnitude number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. mag B-V B-V colour index number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. mag U-B U-B colour index Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. mag n_UBV Flag on the number of measurements: S = Standard star / = Number is unknown * = the minimum number of measurements is given number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. --- o_UBV Number of measurements number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. --- r_UBV Reference key (see file refs.dat) number= the components are indicated by an extra digit; "D" stands for double "Q" for obvious misidentifications (two incompatible measurements of the same star in the same paper) "S" to "U" designates supplementary stars (example in Praesepe, KW 250 and KW 250s both exist) number= The star 100001202 is written as 100012022D, pushing the D into the field reserved for V. This has been left since the field is an A format field. The D is explained in the note on Rem. number= Two stars have values of U-B that appear to be in errors: 620055740 has U-B = -1.62 900011054 has U-B = -2.23; this star is variable. --- Stars showing significant differences in UBV but not known to be variable LID Code number (see file codes.txt) --- Rem Duplicity as in file "ubv.dat" --- Vmag V magnitude mag B-V B-V color mag U-B U-B color mag n_UBV Flag on the number of measurements, as in file "ubv.dat" --- o_UBV Number of measurements --- r_UBV Reference key (see file refs.dat) --- ErrFlag '*' indicates a known error --- Comment Comment on inconsistency --- References ordered by Number r_UBV Reference number, blank for a continuation record number=1 the first two digits of the reference number is related to the used UBV system: 02xxx BV from Cape UcBV system (Nicolet 1975; Catalogue II/27) 14xxx UBV(E) data from Eggen 37xxx UBViyz, Jennens and Helfer (1975) 08xxx UBV(RI), Johnson standards (Johnson and Morgan 1953) (*) 68XXX UBV(RI), Kunkel and Rydgren (1979) (*) 72XXX UBV(RI), Moffet and Barnes (1979) (*) 73XXX UBV(RI), Neckel and Chini (1980) (*) (*) Various UBVRI systems, see Lanz 1986; Catalogue II/116 --- Text Full reference --- refj.txt References ordered by Journal codes.txt Description of the LID numbering system adc.doc Document of Version 'A' of Catalogue adc.tex Document of Version 'A' in LaTeX Francois Ochsenbein CDS 1995 Jul 11 UNKNOWN UNKNOWN * Sept.1987: version 'A' by Anne C. Raugh (see "adc.doc", or "adc.tex") This version is included on the "Selected Astronomical Catalogs, Vol.1" CD-ROM, directory /photom/ubv * 11-Jul-1995: version 'B' (Francois Ochsenbein, CDS) The format was transformed to be fully compatible with catalogue II/193 (1986-1992 data): "STD" flag moved to column 37. The discrepant values were checked, leading to the following corrections for LID stars (the order is provided within parentheses when several measurements exist for a single star) (corrections already mentioned in version 'A' are preceded by (A)) ------------------------------------------------------------------------ Corrections in "ubv.dat" file ------------------------------------------------------------------------ -006007270 shifted columns (A) -004611571 (2) deleted (was duplicated) -002306322 'I' in column "o_UBV" transformed to '1' (A) 003003360 could not be located in the reference #100, and was deleted; it contained the values: .01 + .42 - .01 2 1 100 (A) 100000886 (1) Reference is 0, not corrected 100025290 shifted columns 100047627D shifted columns 100156201 (3) shifted columns 100208786 (2) shifted columns 100285968 shifted columns (A) 100306247 (2) B-V=0.966 (instead of 9.966) 224670098 (1) B-V=0.0310 (the dot was missing) 251380319 (2) B-V=0.05 (the dot was missing) (A) 5122800921(2) Ref=390 (instead of 3900) (A) 5122800921(3) Ref=401 (instead of 4010) (A) 5122800921(4) Ref=411 (instead of 4110) (A) 620102305 o_UBV=3 (instead of blank) 642002248 shifted columns (A) 920330012 B-V=-0.29 (instead of 18.12) 926752107 B-V=-0.22 (instead of -1.05 which is U-B color) ------------------------------------------------------------------------ Corrections in "ubva.dat" file ------------------------------------------------------------------------ (A) 100159560 (6) Ref=8015 (instead of 80150) and shifted columns 600247163 '+' removed in B-V column ------------------------------------------------------------------------ Corrections in "dubious.dat" file ------------------------------------------------------------------------ 318050165 Deleted, because U-B was not measured in ref. 49 ------------------------------------------------------------------------ Corrections in "refs.dat" file ------------------------------------------------------------------------ (A) 100 Page=221 (instead of 223) (A) 1464 Page=254 (instead of 1272) ------------------------------------------------------------------------ II_122B.xml UBV Photometry of Faint Stars (V>14.5) in the Open Cluster M67 2123A II/123A UBV Photometry of Faint Stars UBV Photometry of Faint Stars (V>14.5) in the Open Cluster M67 V N Frolov J K Ananyevskaya Astronomicheskii Tsirkulyar No. 1432, ??? ??? 1986 1986ATsir1432....5F Stars, faint Photometry, UBV This catalog is the result of a program of photographic photometry. Four plates each were taken of M67 in U, B, and V, and were measured and reduced using the standards of Johnson and Sandage (1955) and Eggen and Sandage (1964). The catalog lists identification, V, B-V, U-B, proper motion, and membership probability for 1,053 stars.
The UBV Photometry of Faint Stars (V>14.5) in the Open Cluster M67 (NGC 2682) (UBV-M67; Frolov and Ananyevskaya 1986) lists UBV photometry of faint stars obtained as part of an investigation of M67. It complements the work of Frolov (1984), which dealt with the brighter stars (V '<' 14.5 mag.) Because most of these objects had no previous photometry, Frolov and Ananyevskaya have obtained UBV photometry for all catalog stars. Four plates were taken in each color using the Schmidt telescope of the Radio Astrophysical Observatory of the Latvian SSR, which were then measured and calibrated using the standards of Johnson and Sandage (1955) and Eggen and Sandage (1964). Frolov and Ananyevskaya (1986) note the following: As there was a lack of the faintest standards we had to add photoelectric UBV magnitudes of five stars determined only by one observation. The mean errors are 0.03, 0.04, and 0.03 mag. for U, B, and V magnitudes, respectively. See Frolov (1984) for further details of the data reduction. Of the 1,053 stars included in this catalog, 172 were determined to be members of M67 on the basis of proper motion and photometry. The catalog is in a single file which lists identification, V, B-V, U-B, relative proper motion, and probability of membership for each of the stars investigated.
The catalog of faint stars in M67 ID UBV-M67 number Number in this catalog (increasing, but not consecutive). --- flag Membership flag Two-character code indicating whether this star is a member of M67 as determined by Frolov and Ananyevskaya (1986): * = Cluster member ** = Possible cluster member (probability < 50%) blank = Not a cluster member --- no_San Sanders number Number of the star in the catalog of Sanders (1977). --- V V mag B-V B-V mag U-B U-B mag uncer Uncertainty flag l if the photometry is uncertain. --- pmX Rel. P. M., X Relative proper motion of the star in x as determined by Sanders (1977), arcsec/a pmY Rel. P. M., Y Relative proper motion of the star in y as determined by Sanders (1977) arcsec/a prob Membership probability (percent) Percentage probability that this star is a member of M67 as determined by Sanders (1977). --- Nancy Grace Roman ADC/SSDOO 1996 Feb 16 The processing of this catalog for the archive and the preparation of the Script document on which this document is based were carried out by Wayne H. Warren Jr. UNKNOWN UNKNOWN The UBV Photometry of Faint Stars (V>14.5) in the Open Cluster M67 (NGC 2682) (UBV-M67) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in December 1986. The original tape consisted of two text files: the first file contained a description of the catalog file and has been incorporated into this document; the second file contained the catalog data. No changes were made to the data file. A FORTRAN program was run to check the validity of each field according to its data type and value. II_123A.xml Catalogue of UBV Photometry and MK Spectral Types in Open Clusters (3rd Edition, August 1986) 2124A II/124A UBV and MK types in Open Clusters, 3rd ed. Catalogue of UBV Photometry and MK Spectral Types in Open Clusters (3rd Edition, August 1986) J -C Mermilliod Astron. Astrophys. Suppl. Ser. 24 159 1986 1976A&AS...24..159M Clusters, open MK spectral classification Photometry, UBV The catalog is a compilation of UBV photoelectric photometry and MK spectral types published up to 1986 for 16433 stars in 295 open clusters. It updates the 1976 edition and contains nearly twice as many data as the earlier version. The catalog lists identifications, cross-identifications, V, B-V, U-B, spectral types, remarks on various peculiarities, and references.
The Catalogue LID Identification in Geneva/Lausanne system number=1 see Mermilliod, Bull. Inf. CDS 14, 32 (1978) for a description of the numbering system; detailed references are in file "lid.txt". --- n_LID Remark about star number=2 this peculiarity is a single-character code as follows: B = Spectroscopic Binary P = Peculiar star D = Visual binary V = Variable star E = Emission-line star --- OrigID Original identification as listed in reference for the data --- pmID Identification as listed in proper motion study --- HD Henry Draper Catalog (HD) number --- DM Durchmusterung catalog ID number=3 The Durchmusterung number has the form 'nn+ZZNNNNN' where nn = 'BD', 'CD', 'CP' +ZZ = zone in degrees NNNNN = number in the zone --- Vmag V magnitude in the UBV system mag B-V B-V color in the UBV system mag U-B U-B color in the UBV system mag r_UBV Photometry reference number --- MKtype Spectral type --- r_MKtype Spectral type reference number --- Remarks Remarks and further cross-identifications (details in "adc.doc" or "adc.tex") --- All references as a single file RefNum Reference number --- n_RefNum 'P' for Photometry ref. ("r_UBV" in catalog.dat),'S' for Spectrosc. ref. ("r_MKtype in catalog.dat) --- Ref Text of bibliographic reference --- adc.doc ADC Documentation (ASCII) adc.tex ADC Documentation (LaTex) lid.txt Description of LID numbers (Lausanne/Geneve) refmk.txt References for Spectral Classification refubv.txt References for Photometry Francois Ochsenbein CDS 1995 Apr 11 UNKNOWN UNKNOWN See in "adc.doc" or "adc.tex", section 3 (History), from the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory /photom/ubvopen II_124A.xml IRAS Serendipitous Survey Catalog 2126 II/126 IRAS Serendipitous Survey Catalog IRAS Serendipitous Survey Catalog S G Kleinmann R M Cutri E T Young F J Low F C Gillett Joint IRAS Science W.G. ??? ??? 1986 1987issc.book.....K Infrared sources Photometry, infrared Surveys This is a catalog of 12, 25, 60 and 100 micron photometric observations of 43,866 point-like sources detected fortuitiously in the Infrared Astronomical Satellite Pointed Observation program. The main objective was to take advantage of the longer-than-nominal integration time per source to extend the detection threshold relative to that of the Point Source Catalog (PSC); about three-fourths of the Serendipitous Survey Catalog (SSC) sources do not appear in the PSC. From 1813 Pointed Observation fields, the effective sky coverage is 1108 square degrees. Relative to the PSC, the SSC is characterized by: enhanced sensitivity (by a factor of about 4) in all four wavelength bands; excellent reliability in uncrowded fields; uneven sky coverage and completeness; reduced positional accuracy; improved photometric accuracy; much greater depth in crowded fields at the expense of reliability and accuracy. The SSC data processing, the catalog format, and an analysis are given in the Explanatory Supplement to the IRAS Serendipitous Survey Catalog.
Information about the reference and confirming grids (observations) in which point sources were identified FNAME Field Name (1) (2) The IRAS/SSC field name is the position of the center of the reference grid, given in the form hhmmssSddmmss. --- RGRID Reference Grid No. (2) The reference grid has the lower 60 um median noise. --- RDATE Observation Date of RGRID (2) (JD 2445000 +) JD CGRID Confirming Grid No. number=2 This quantity is listed in the printed version of the catalog. --- CDATE Observation Date of CGRID (2) (JD 2445000 +) JD MACRO Macro Type (2) number=3 Macro code is (Table II.A of "Explanations") ------------------------------------------------------ Code Name Scans Length Cross-step SNR Gain arcmin arcmin improvement ------------------------------------------------------ A DPS02B 6 96 0.3 4.8 B DPS05B 3 360 1.0 3.5 C DPS52B 6 96 0 4.8 D DPS55B 3 360 0 3.5 E DPS60B 4 60 0.8 4.0 F DPS60D 5 48 0.4 4.4 G DPS61C 12 48 0.2 6.9 H DPS61D 15 48 0.2 7.7 I DPS62D 9 96 0.4 6.0 J DPS63D 3 96 0.8 3.5 K DPS60C 5 48 0.4 4.4 L TPS52B 6 96 0 4.8 M DPS60M 5 48 0.4 4.4 ------------------------------------------------------ --- GLON Galactic Longitude number=2 This quantity is listed in the printed version of the catalog. deg GLAT Galactic Latitude number=2 This quantity is listed in the printed version of the catalog. deg PDRAS Sign of R.A. Difference between Grid centers --- PDRA Amplitude of R.A. Diff. between Grid Centers arcsec PDDECS Sign of Dec. Difference between Grid Centers --- PDDEC Amplitude of Dec. Diff. between Grid Centers arcsec RANGLE Reference Grid Scan Direction (E of N) deg CANGLE Confirming Grid Scan Direction (E of N) deg EFFAREA Effective Area of Grid Overlap (2) covered by both the reference and confirming grids (in 0.01 square degrees). 0.01deg2 RUNDF No. of additional grid pairs with Overlap > 5% number=2 This quantity is listed in the printed version of the catalog. --- RNOISE Median Noise of Ref. Grid (1 value per band) mJy CNOISE Median Noise of Conf. Grid (1 value per band) mJy NSOURC Number of Confirmed Sources (1 value per band) --- NCONF Number of Confused Confirmations (2) (1 value per band) --- CIRRUS Number of 100 um only Confirmed Sources number=2 This quantity is listed in the printed version of the catalog. --- NMERGE Number of Merged Sources, i.e. number of source records following the field header. --- Properties of the point sources identified NAME IRAS/SSC Source Name number=1 Sources are listed in order of increasing Right Ascension within each field. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAds Right Ascension 1950 (seconds) 0.1s DE- Declination 1950 (Sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec ANGLE Position Angle of SSC Source Error Box expressed in degrees East of North. --- FLUX Averaged Non-color Corrected Flux Densities(2) (1 value per band) (1Jy = 10-26 W/m2/Hz) Jy FQUAL Flux Density Quality (2) high-quality=3, moderate quality=2, upper limit =1 (1 value per band) --- RGRID Reference Grid Number --- RELUNC Percent Relative Flux Density (2) Uncertainties (1 value per band) % TLSNR 10x Local Signal-to-Noise Ratio (1 value per band) --- CC Point Source Correlation Coefficient (2) between 70-100%. These are encoded as alphabetic characters with A=100, B=99..Z=75-70 (1 value per band) The quoted correlation coefficients come from the reference or confirming grids, whichever is higher, for high quality sources. --- TRFLUX 10x Fc/Fr (confirmed/reference)i (1 value per band) SSC sources can have flux density ratios 0.5 < Fc/Fr < 2.0. --- POSDRS12 Right Ascension Delta Sign (12 um) --- POSDR12 Right Ascension Delta arcsec POSDDS12 Declination Delta Sign --- POSDD12 Declination Delta arcsec POSDRS22 Right Ascension Delta Sign (25 um) --- POSDR22 Right Ascension Delta arcsec POSDDS22 Declination Delta Sign --- POSDD22 Declination Delta arcsec POSDRS32 Right Ascension Delta Sign (60 um) --- POSDR32 Right Ascension Delta arcsec POSDDS32 Declination Delta Sign --- POSDD32 Declination Delta arcsec POSDRS42 Right Ascension Delta Sign (100 um) --- POSDR42 Right Ascension Delta arcsec POSDDS42 Declination Delta Sign --- POSDD42 Declination Delta arcsec PNEARC Number of Sources in Confusion Window (2) (3) (1 value per band) --- NID Number of Positional Associations number=2 This quantity is listed in the printed version of the SSC. --- IDTYPE Type of Object number=2 This quantity is listed in the printed version of the SSC. --- Information about positional associations with sources in other catalogs CATNO Catalog Number number=1 For associations with the IRAS/PSC, this value is 41. --- SOURCE Source ID --- TYPE Source Type/Spectral Class number=2 For associations with the IRAS/PSC, this field is left blank. --- RADIUS Radius Vector from SSC Position to Association arcsec POS Position Angle from SSC Position to Association (E of N) deg FIELDl Object Field #1 Dependent number=3 For associations with the IRAS/PSC, this value is a flag indicating the bands in which the source was detected with medium or high quality; it is encoded as indicated in the PSC Supplement Table X.B.2. --- FIELD2 Object Field #2 Dependent number=4 For associations with the IRAS/PSC, this value is the PSC 2.0 Flux Density in the shortest (first) wavelength band in which it was detected. Flux Densities higher than 10 Jy are encoded 9999. --- FIELD3 Object Field #3 Dependent number=5 For associations with the IRAS/PSC, this value is the PSC 2.0 Flux Density in the second wavelength band in which it was detected. Flux Densities higher than 10 Jy are encoded 9999. --- NAME SSC Name association number=6 These fields are a repetition of bytes 1-11 and 71-75 of "sources" table. --- RGRID SSC Name association number=6 These fields are a repetition of bytes 1-11 and 71-75 of "sources" table. --- Overlapping fields (Appendix A) GRID0 Reference Grid No. number=1 If a Reference Grid is overlapped (>5% of area) by more than six grids, the list of overlapping grids grids is continued in succeeding records. In this case, bytes 1-6 of each continuation record are blank. --- GRID1 First overlapping grid no., >5% overlap with Reference Grid --- OVLP1 Overlapping area (First and Ref.) arcmin2 GRID2 Second overlapping grid, >5% overlap with Ref. --- OVLP2 Overlapping area (Second and Ref.) arcmin2 GRID3 3rd overlapping grid, >5% overlap --- OVLP3 Overlapping area arcmin2 GRID4 4th overlapping grid, >5% overlap --- OVLP4 Overlapping area arcmin2 GRID5 5th overlapping grid, >5% overlap --- OVLP5 Overlapping area arcmin2 GRID6 6th overlapping grid, >5% overlap --- OVLP6 Overlapping area arcmin2 meaning.txt Details of association catalogues ssc.doc Information about interpretation of catalog entries, from the Explanatory Supplement to the IRAS Serendipitous Survey Catalog, Francois Ochsenbein CDS Seth Digel SSDOO/ADC 1997 Aug 14 II_126.xml A Study of Visual Double Stars with Early-Type Primaries. IV. Astrophysical Data 2127 II/127 Visual Double Stars with Early-Type Primaries. IV A Study of Visual Double Stars with Early-Type Primaries. IV. Astrophysical Data K P Lindroos Astron. & Astrophys. Suppl. 60 183 1985 1985A&AS...60..183L Photometry, uvby, beta Stars, double and multiple Astrophysical parameters (MK class, colour excess, absolute magnitude, distance, effective temperature, mass and age) are derived from calibrations of the uvbybeta indices for the members of 253 double stars with O or B type primaries and faint secondaries. The photometric spectral classification is compared to the MK classes and the agreement is very good. The derived data together with spectroscopic and JHKL data indicate that these stars are likely to be members of physical systems. For 90% of the physical pairs the projected separations between the components is less than 25,000 AU. A majority of the physical secondaries are late type stars and 50% of them are contracting towards the zero-age main-sequence (ZAMS).
Data HD HD number When data on several components is given, each component occupies a separate record. When the HD column is blank, the HD number is the same as for the preceding record. --- Comp Component designation as given in Paper II An asterisk (*) following the component designation of composite primaries indicates that the magnitude difference is less than 4.0 --- rel Relation between secondary and primary PH = Physical secondary OPT = Optical secondary ? = Undecided Uncertain cases are indicated by a "?" following the most likely relation. Numbers refer to which of the criteria the classification is based upon. A secondary is classified as an optical component if any of the following criteria is fulfilled: 1 = The absolute magnitude Mv' places the star more than 0.5 mag below the ZAMS at (b-y)', (or at the (b-y)0 corresponding to the spectral type). Primaries noted to be spectroscopic binaries have been corrected for equally bright components. 2 = Mv' is inconsistent with the MK classification. 3 = (b-y)' (or c' for B stars) inconsistent with the MK classification. 4 = For stars earlier than G0 the difference between Mv' and Mv(beta) or Mv(c') is larger than 1.0 mag. 5 = The indices m', c' and beta are inconsistent with the MK class corresponding to (b-y)' and Mv'. 6 = The components have different radial velocities in Paper III. 7 = Astrometric data show that the system is optical. 8 = Some secondaries which did qualify as physical companions by the criteria above were still considered as optical if their position in the HR diagram would be in serious conflict with the evolutionary tracks and the assumption of coeval formation of the primary and secondary. --- Sp1 MK class from Paper I or from literature --- paren1 Parentheses --- Sp2 MK class estimated from photometric indices d = dwarf g = giant --- paren2 Parentheses --- E(b-y) Colour Excess: if negative, assumed to be 0 mag mag Absolute magnitude mag Hmag Height above 0-age main sequence mag lnLum Logarithm of the luminosity solLum lnTeff Logarithm of the effective temperature --- l_Age Indicates upper limit of Age --- Age Age of the primary Ma Mass Mass for primary solMass Dist Distance pc Sep Projected separation between PH and primary AU rem1 Remarks C = According to Age the star is still contracting with respect to ZAMS. SB = Spectroscopic binary --- rem2 Indicates a note in Paper IV --- Notes on Individual Stars HD "HD" --- HDnum HD number of star --- Comp Component(s) --- colon Separator Blank in this byte indicates that text is continued from previous record. --- text Note on individual star from Astron. & Astrophys. Suppl. 60, 183. --- Julie Anne Watko SSDOO/ADC 1996 Apr 10 II_127.xml Photometric Data for the Bright Stars 2128 II/128 Photometric Data for the Bright Stars Photometric Data for the Bright Stars B Hauck M Mermilliod Bull. Inform. CDS, No. 31 ??? ??? 1986 1986BICDS..31..131H Photometry Stars, bright References are given to the photometric data available for 9008 stars in the Bright Star Catalog.
A new (1986) version of the General Catalogue of Photometric data (Hauck et al., 1986) was used to establish a file that indicates the systems in which a star belonging to the Bright Star Catalogue (Hoffleit and Jaschek, 1982) has been measured. Fourteen novae or extended sources were excluded. Two binary systems have separate entries in the BSC but cannot be resolved photometrically. There is no photometric data for 86 stars.
The main catalog HR Bright Star (HR) number --- ast Meaning of asterisk unknown --- HD HD number --- note Asterisk indicate note in BSC --- d Double star component D = double star with components measured as one 1 = brighter component 2 = fainter component --- v Indicates a variable magnitude --- V V magnitude mag ref References --- Key to the references for data ref_no Number of reference --- color Color systems included --- ref Reference (copy references minus Hoffleit ) --- no Number of stars from reference --- Nancy Grace Roman ADC/SSDOO 1996 Jan 05 II_128.xml Automated Two-Dimensional Classification from Multicolour Photometry in the Vilnius System 2130 II/130 2-D Classification, Vilnius Photometry M56 Region Automated Two-Dimensional Classification from Multicolour Photometry in the Vilnius System F Smriglio R P Boyle V Straizys R Janulis K Nandy H T MacGillivray A McLachlan R Coluzzi C Segato Astron. Astrophys. Suppl. Ser. 66 181-190 1986 1986A&AS...66..181S Photometry, classification Photometry, Vilnius This catalogue gives the seven-color photometry in the Vilnius system stars and two-dimensional classification of 752 stars. Photographically determined magnitudes obtained by COSMOS (MacGillivray and Stobie 1984) on the Schmidt plates were input into software described by Smriglio et al. (1986) as a method of automated two-dimensional stellar classification in the Vilnius seven-color intermediate band photometric system (Straizys and Zdanavicius 1970). A region of approximately two square degrees in Lyra centered on RA (1950) = 19 h 14.6 min, DE (1950) = 30 deg 05 arcmin in the direction of the globular cluster M56 was studied and the two-dimensional classification of 752 stars in the magnitude range V = 11 to 15 mag was studied. The photo- metric system, the method of reduction, the classification procedure and errors were described by Smriglio et al. (1986). The number of stars for which all the six color indices in the Vilnius system are available is close to 3000, but the number of stars which have received two dimensional classi- fication is 752. The success rate of classification appears to be high for stars brighter than V = 15.0 mag for which photometric accuracy is better than +-5%.
Data ID Running number --- RAh Right Ascension (1950.0) hours h RAm Right Ascension (1950.0) minutes min RAs Right Ascension (1950.0) seconds s DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin DEs Declination (1950.0) arcseconds arcsec V V magnitude mag U-P U-P color index mag P-X P-X color index mag X-Y X-Y color index mag Y-Z Y-Z color index mag Z-V Z-V color index mag V-S V-S color index mag Sp Spectral type --- L Luminosity class d = dwarf g = giant c = supergiant --- Julie Anne Watko SSDOO/ADC 1996 May 30 II_130.xml A catalog and identification charts of the Pleiades Flare stars 2131 II/131 Tonantzintla Pleiades Flare Stars A catalog and identification charts of the Pleiades Flare stars G Haro E Chavira G Gonzalez Bol. del Instituto Tonantzintla, 3, N. 1 ??? ??? 1982 1982BITon...3....3H J/ApJS/85/315 : F, G and K dwarf stars of the Pleiades (Soderblom+ 1993) Hertzsprung E., 1947, Ann. Sternw. Leiden, 19, 1 (=1947AnLei..19a...1H) Jones O.F., 1973, Astron. Astrophys., Suppl. Ser., 9, 313 (=1973A&AS....9..313J) Van Maanen A., 1945, Astrophys. J., 102, 26 (=1945ApJ...102...26V) Clusters, open Stars, flare The original catalog lists the flare stars discovered by different astronomical observatories over an area slightly larger than 20 square degrees in the Pleiades regions centered on Alcyone. Not all the flare stars are members of this cluster, membership indicators are provided in the catalog. The catalog, combining Tables 1 and 2 of the publication, gives the data for 1531 flares of 519 flare stars. Nomenclature Notes: The flare stars from this paper (column "TonF" in the "catalog" file) are found in the literature as "Ton", or "HCG", which are both ambiguous.
The Catalog of the Pleiades Flare stars TonF Tonantzintla serial number --- n_TonF The '*' indicates the entry with the first flare-up discovered --- FlareNo Flare-up running number for a given star --- m_FlareNo Letter A, B,... for different registrations of the same flare-up --- Flare Original flare-up designation number=1 the following abbreviations designate Observatories: Asiago (A), Abastumani (AB), Byurakan (B), Konkoly (K,K*), Konkoly-Byurakan(KB), Mt Palomar (P), Rojen (R), Sonneberg (S), and Tonantzintla (T). J&M is for Johnson and Mitchell. --- Hertz Hertzsprung (1947) or Van Maanen (1945) star number when availablE --- RAh Right Ascension 1900 (hours) h RAm Right Ascension 1900 (minutes) min DE- Declination 1900 (sign) --- DEd Declination 1900 (degrees) deg DEm Declination 1900 (minutes) arcmin ObsDate Date of Observation (day month year) --- l_minMag Uncertainty flags on minMag number=2 the uncertainty flags are coded as follows: '(', ':', '=:' (approximately equal to), '>', '>=', '>=:' --- minMag Flare star magnitude at minimum in U or pg mag n_minMag Band of minMag: blank for pg, or 'U' --- l_DmU Uncertainty flags on DmU number=2 the uncertainty flags are coded as follows: '(', ':', '=:' (approximately equal to), '>', '>=', '>=:' --- DmU Amplitude observed in U band mag l_DmB Uncertainty flags on DmB number=2 the uncertainty flags are coded as follows: '(', ':', '=:' (approximately equal to), '>', '>=', '>=:' --- DmB Amplitude observed in B, V or pg band mag n_DmB Band of DmB: blank for pg, 'B' or 'V' --- l_minDm Uncertainty flags on minDm number=2 the uncertainty flags are coded as follows: '(', ':', '=:' (approximately equal to), '>', '>=', '>=:' --- minDm Minimum amplitude observed in U or pg band mag n_minDm Band of minDm: blank for pg, or 'U' --- l_maxDm Uncertainty flags on maxDm number=2 the uncertainty flags are coded as follows: '(', ':', '=:' (approximately equal to), '>', '>=', '>=:' --- maxDm Maximum amplitude observed --- n_maxDm Band of maxDm: blank for pg, or 'U', 'B', 'V' --- Nbursts Number of different outbursts observed --- Member Membership (' M') or non-membership ('N-M') in the Pleiades according to Hertzsprung (1947) --- Pr Membership probability values according to Jones (1973) --- SpType Spectral Type --- Chart Number of identification chart in the original printed version --- NoteFlag 'N' indices a note in file "notes" --- RefNo Number of reference in file "refs" --- m_RefNo Letter A,B,... for different references WITH the same number --- Notes to catalog N/R Note indicator --- TonF Tonantzintla serial number --- Text Text of note, or reference --- References quoted in catalog and notes N/R Reference indicator --- RefNo Reference number --- m_RefNo Letter A,B,... for different references with the same number --- Text Text of reference --- Francois Ochsenbein CDS 1996 May 03 UNKNOWN UNKNOWN The electronic version of the Tonantzintla catalogue of the Pleiades flare stars was prepared by M.K. Tsvetkov, K.Y. Stavrev, and K.P. Tsvetkova, at the Department of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, in June 1987. This standardized documentation has beed added at CDS, in May 1996. II_131.xml Catalog of magnetic field measurements 2134 II/134 Catalog of Magnetic Field Measurements Catalog of magnetic field measurements P Didelon Astron. and Astroph. Supp. 53 119 1983 1983A&AS...53..119D Magnetic fields The catalog contains references to all measurements of stellar magnetic fields published in the literature between 1958 and 1981. The catalog provides for each object identifications, position, magnitude, period, extrema of the magnetic field measured, number of measurements, method used, spectral type, bibliographic references, and notes.
Users should be aware of possible differences between results obtained with different techniques, so that the measurements given here should not be used without detailed examination to derive, for instance secular variations.
The compilation of magnetic fields HD HD Identification --- m_HD Suffix to HD A = primary component of binary B = secondary component of binary I = blend of two entries --- Name Alternate Identification --- RAh Right Ascension (1950.0) hours Equatorial coordinates of the star for 1950.0 taken from the CDS database or from McCook and Sion (1977, Cat. <III/129>). h RAm Right Ascension (1950.0) minutes min DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin Vmag Visual Magnitude Visual Magnitude as given by the author. If not available in the reference, it is taken from the CDS database or from McCook and Sion (1977, Cat. <III/129>). mag n_Period Note on Period > = lower limit of Period is listed ? = low accuracy value of Period # = very low accuracy value of Period --- Period Magnetic or Spectroscopic Period d Code Code Regarding Field H = well established field P = probable Q = questionable U = unmeasurable N = no field detected even with sharp line or small error value --- Sp Spectral Type in Reference --- Hmin Minimum Value of Field 10-4T u_Hmin Uncertainty flag on Hmin --- Hmax Maximum Value of Field 10-4T Nobs Number of Measurements --- Tech Code for Measurement Technique Techniques of measurement of effective field H(eff) = Photographic technique based on Zeeman Spectrograms (refs. 1, 5,...) PPZ = Photoeletric polarimetry technique for detection of Zeeman effect by polarization in line wings (refs. 39, 40, 53...) MLP = Multiple line polarization; same technique as PPZ but the measurement is made for several lines at the same time (refs. 113, 148) RZM = Reticon Zeeman measurement; same technique as the photographic one but with a reticon detector (refs. 94, 97) CCP = Continuum circular polarization measurements in strong field, mainly used for white dwarfs (refs. 55-150) Techniques of measurement of transverse field H(T) CLP = Continuum linear polarization measurements in very strong fields (H > 50 MG) give transverse magnetic field (ref. 133) LPL = Linear polarization in line detects transverse magnetic field (refs. 84, 106, 155, 156, 157). No value of the field is calculated, but the strong dependence of the polarization diagram on the field geometry can improve the determination of parameters and give the orientation of the spin axis of the star in space. See calculations for the Ap star 53 Cam in Borra (1973ApJ...186..959B), Finn and Kemp (1974MNRAS.167..375F) and Landi Degl'Innocenti et al. (1981ApJ...249..228L), and tables of linear polarization for the interpretation of observations in Landi Degl'Innocenti (1982A&A...110...25I) and the note to reference 99 (in printed article only) Techniques for measurement of the surface field H(S) RZP = Resolved Zeeman patterns; high-resolution spectroscopy without Zeeman analyzer (refs. 17, 18, 21, 23...) LWE = Correlation between line equivalent width or line strength and surface field (refs. 29, 33, 86) DMB = Differential magnetic broadening or deformation of line profiles, between sensitive and insensitive magnetic lines. Used with a Fourier deconvolution technique this method gives the percentage of surface covered by the field (filling factor) (refs. 93, 114, see also Robinson 1980ApJ...239..961R and Marcy, 1982) WPP = Wide-band photoelectric polarimetry and computer models can give an estimation of the surface field (ref. 99) IML = Intensification of magnetic lines (ref. 109) CRF = Cyclotron resonance frequency can explain some emission or absorption features whose circular and linear polarizations are of the same order, some strange variations of these, and can give the surface field for the fundamental cyclotron radiation frequency (refs. 142 and 136, 138, 143...) --- r_Hmin Bibliographic Reference Number --- rem Note code (see Published Cat.) --- Sp2 Spectral Type in M. Jaschek <Cat. III/42> --- References ref Bibliographic Reference Number --- aut Authors --- bibcode Journal, Volume, Page, as 19-digit bibcode when possible. --- Francois Ochsenbein CDS 1998 Aug 24 UNKNOWN UNKNOWN * 21-Feb-1996: the catalogue documentation was written by Julie Anne Watko [SSDOO/ADC] * 24-Aug-1998: reformatting at CDS (F. Ochsenbein): - magnetic field values reformatted in file data.dat to have values on a uniform scale, - bibcodes added in file refs.dat. II_134.xml Supplement to the Catalogue of Diffuse Interstellar Band Measurements 2135 II/135 Suppl. to Diffuse Interstellar Band Measurements Supplement to the Catalogue of Diffuse Interstellar Band Measurements J Guarinos CDS Inf. Bull. No. 34, p. 141 ??? ??? 1988 1988BICDS..34..141G II/149 : Catalog of Diffuse Interstellar Band Measurements (Snow+ 1977) Interstellar medium Spectroscopy This bibliographic search has been undertaken in order to gather all data concerning four diffuse interstellar bands (DIB) published since the Snow, York, and Welty (1977) catalogue, and up to 1987.0. These four DIB are : 4430, 5780, 5797, and 6284 Angstrom. In the present set of data, no statistical reduction to a unique system has been made because most of the lists contain only few data.
The diffuse interstellar band Supplement Name Designation of the star number=1 We have given HD numbers whenever possible, and if these were unavailable, Durchmusterung numbers (BD, CD, or CPD). The cross-identification comes from the SIMBAD data base. If neither HD nor DM numbers exist, the designation used by the author was kept. AzV comes from Azzopardi and Vigneau (1975A&AS...22..285A, Cat. <V/13>). Wray 15 comes from Wray, Univ. Microfilm Inc. Ann Arbor Michigan, Table 15. --- Snow Exists in Snow et al., Cat. <II/149> --- GLON Galactic longitude number=3 the position is unknown for 6 stars, in VI Cyg (Cyg OB2 association) and in the cluster Berkeley 87 deg GLAT Galactic latitude number=3 the position is unknown for 6 stars, in VI Cyg (Cyg OB2 association) and in the cluster Berkeley 87 deg W4430 Equivalent width (in mA) of 4430A line 0.1pm e_W4430 Standard error on W4430 0.1pm f_W4430 if e_W4430 is just an estimate --- W5780 Equivalent width (in mA) of 5780A line 0.1pm e_W5780 Standard error on W5780 0.1pm f_W5780 if e_W5780 is just an estimate --- W5797 Equivalent width (in mA) of 5797A line 0.1pm e_W5797 Standard error on W5797 0.1pm f_W5797 if e_W5797 is just an estimate --- W6284 Equivalent width (in mA) of 6284A line 0.1pm e_W6284 Standard error on W6284 0.1pm f_W6284 if e_W6284 is just an estimate --- Ac4430 Central depth of the continuum at 4430A % e_Ac4430 Mean error on Ac4430 % Ac5780 Central depth of the continuum at 5780A % Ac5797 Central depth of the continuum at 5797A % Ac6284 Central depth of the continuum at 6284A % E(B-V) Colour excess in the UBV system. mag Vmag V magnitude. mag SpType MK type. --- Ref Reference number=2 References codes are: 1: Schmidt (1978ApJ...223..458S) 2: Meyer (1983ApJ...266L..51M) 3: Kumar, Federman, Vanden Bout (1982ApJ...261L..51K) 4: Chlewicki, et al. (1986ApJ...305..455C) 5: Whittet, Blades (1980MNRAS.190p..41W) 6: Walborn (1977PASP...89..765W) 7: Somerville, Blades (1980MNRAS.192..719S) 8: Houziaux, Nandy, Morgan (1985MNRAS.215p...5H) 9: Snow, Timothy, Saar (1982ApJ...262..611S) 10: Blades, Somerville (1981MNRAS.197..543B) 11: Baines, Whittet (1983MNRAS.203..419B) 12: Tug, Schmidt-Kaler (1981A&A....94...16T) 13: Hutchings (1980PASP...92..592H) 14: Federman, Kumar, Vanden Bout (1984ApJ...282..485F) 15: Kumar (1986ApJ...306...38K) 16: Snell, Vanden Bout (1981ApJ...244..844S) 17: Isobe, et al. (1986PASJ...38..511I) --- Francois Ochsenbein CDS 1997 Feb 28 J. Guarinos would like to thank Pr. C. Jaschek who suggested this update, and Mme F. Boisselier for the typing. UNKNOWN UNKNOWN * The catalogue was keypunched at CDS under the control of J. Guarinos. in 1988. * The description was added by Julie Anne Watko [ADC] in May 1996. * The "catalog" file was reshaped, checked and documented in February 1997 at CDS (Francois Ochsenbein), thanks to the original documents written by J. Guarinos. II_135.xml Predicted K Magnitudes for Stars in the Regions South of Declination -33 deg. and North of +81 deg. 2141 II/141 Predicted K Magnitudes for Polar Stars Predicted K Magnitudes for Stars in the Regions South of Declination -33 deg. and North of +81 deg. Y -J Kuan Unpublished thesis, ??? ??? 1988 1988 Magnitudes A list of 2399 stars predicted to be brighter than K = +3.00 in the regions of the sky not surveyed by the Two-Micron Sky Survey (IRC) is presented. Relations between V-K color and spectral types have been derived and employed to predict K for visually bright BS and SAO stars. K-[12mu] color/spectral type relations have been obtained and used to predict K for IRAS/PSC sources associated with BS or SAO stars. For visually faint, unidentified PSC sources, criteria have been developed to separate the stellar sources from the non-stellar ones. The [12mu]-[25mu] versus [25mu]-[60mu] color-color diagram has been used to classify PSC sources and the mean K-[12mu] colors of stars of different classes have been used to predict K for unidentified PSC stellar sources.
The data RAh Right Ascension hours (1950.0) h RAm Right Ascension minutes (1950.0 min RAs Right Ascension seconds (1950.0 s DE- Declination sign (1950.0) --- DEd Declination degrees (1950) deg DEm Declination minutes (1950.0) arcmin DEs Declination seconds (1950.0) arcsec SAO SAO number --- SAO_sp SAO spectral type --- SAO_v SAO visual magnitude mag SAO_K K magnitude predicted from SAO mag HR Bright Star Catalog (BSC) num. --- HR_sp BSC spectral type --- HR_spe Emission star denoted by E --- HR_lum Lum.Cl.(Arabic) Compos. spect=C Subgiants are denoted by 3 or 5 Class I = 0 No luminosity given = 6 Ia = A Ib = B --- HR_V V magnitude from BSC mag HR_K K magnitude predicted from BSC mag IRAS IRAS PSC number --- IRAS_12 12 micron from IRAS mag SAO_PSC SAO number predicted from PSC --- K_S/P K mag. from SAO/PSC comparison mag HR_PSC HR number predicted from the P --- K_H/P K mag. from HR/PSC comparison mag PSC_K K mag for PSC faint stars mag cat Code for other cat. assoc. 1 = General Catalog of Variable Stars (Kukarkin et al., 1969=1971) 2 = Dearborn Survey of Faint Red Stars (Lee et al., 1947) 7 = SEL (Wackerling, 1970) 16 = CSV (Kukarkin et al., 1982) 17 = CCS (Stephenson, 1973) 18 = Catalog of Nearby Stars (Gliese, 1969) 19 = CSS (Stephenson, 1976) --- conf Flux and confusion criteria 1 = [12mu] le 2.70 2 = no other extended sources in the region 3 = source probably not part of an extended source 4 = probably no extended structure in region at 12 microns 5 = probably no extended structure in region at 25 microns 6 = no confusion flag set at 12 microns 7 = no confirmed sources nearby 8* = 12 mu flux gt 25 mu flux gt 60 mu flux 9 = flux quality at 12 mu is high 10* = 12 mu flux gt 25 mu flux 11 = 25 mu flux ge 60 mu flux 12 = not associated with extragalactic objects only 13* = [12mu]-[25mu] le 2.68 and [25mu]-[60mu] le 1.38 --- c_ran Color range 1 = [12mu]-[25mu] gt 0.2 2 = [12mu]-[25mu] gt 0.7 3 = [12mu]-[25mu] gt 0.2 and lt 1.2 4 = [12mu]-[25mu] gt 1.2 --- Nancy G. Roman ADC/SSDOO 1995 Apr 24 II_141.xml Catalogue of the brightest stars in the field of M31 2144 II/144 Brightest stars in the field of M31 Catalogue of the brightest stars in the field of M31 E M Berkhuijsen R M Humphreys F D Ghigo W Zumach Astron. Astrophys. Suppl. Ser. 76 65 1988 1988A&AS...76...65B II/145 : for the foreground stars. J/A+A/214/68 : Berkhuijsen E.M., Humphreys R.M.: 1989 Bull. Inf. Centre Donnees Stellaires, 36, 179-180 (1989) Regional catalog This Catalogue of 11438 stars in the field of M31 is based on a set of Tautenburg Schmidt plates in U, B, V and R taken by van den Bergh. The range of visual magnitudes of stars is 11.5 < V < 20.
Stars in M31 field DecStrip Declination strip deg Sequence Number within DecStrip --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec x_Vmag 'B' if B magnitude given --- Vmag V magnitude, unless x_Vmag specifies that B is given mag e_Vmag mean error on V mag q_Vmag 'm' indicating a marginal Vmag --- (U-B) colour index mag e_(U-B) Mean error on (U-B) mag q_(U-B) 'm' indicating a marginal (U-B) --- (B-V) colour index mag e_(B-V) Mean error on (B-V) mag q_(B-V) 'm' indicating a marginal (B-V) --- (V-R) colour index mag e_(V-R) Mean error on (V-R) mag q_(V-R) 'm' indicating a marginal (V-R) --- CDS 1993 May 28 UNKNOWN UNKNOWN The original (non-standard) FITS table has been converted into a standard ASCII file at CDS II_144.xml A catalogue of the brightest stars in a foreground field of M31 2145 II/145 Brightest stars in a foreground field of M31 A catalogue of the brightest stars in a foreground field of M31 E M Berkhuijsen R M Humphreys F D Ghigo W Zumach Astron. Astrophys. Suppl. Ser. 76 65 1988 1988A&AS...76...65B II/44 : for stars in the field of M31. J/A+A/214/68 : Berkhuijsen E.M., Humphreys R.M.: 1989, Bull. Inf. Centre Donnees Stellaires, 36, 179-180 (1989) Regional catalog Catalogue of 8778 stars in a foreground field based on a set of Tautenburg Schmidt plates in U, B, V and R taken by van den Bergh. The range of visual magnitudes of stars is 11.5 < V < 20.
Foreground stars in M31 field DecStrip Declination strip number deg Sequence Number within DecStrip --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec x_Vmag 'B' if B magnitude given --- Vmag V magnitude, unless x_Vmag specifies that B is given mag e_Vmag mean error on V mag q_Vmag 'm' indicating a marginal Vmag --- (U-B) colour index mag e_(U-B) Mean error on (U-B) mag q_(U-B) 'm' indicating a marginal (U-B) --- (B-V) colour index mag e_(B-V) Mean error on (B-V) mag q_(B-V) 'm' indicating a marginal (B-V) --- (V-R) colour index mag e_(V-R) Mean error on (V-R) mag q_(V-R) 'm' indicating a marginal (V-R) --- CDS 1993 May 28 UNKNOWN UNKNOWN The original (non-standard) FITS table has been converted into a standard ASCII file at CDS II_145.xml A List of Observations of the Ap Star HR 1217 from 1980 to 1986 2146 II/146 Observations of the Ap Star HR 1217 from 1980-86 A List of Observations of the Ap Star HR 1217 from 1980 to 1986 D W Kurtz P Martinez J Seeman J M Matthews M Cropper J C Clemens T J Kreidl C Sterken H Schneider W W Weiss S D Kawaler S O Kepler A van der Peet D Sullivan H J Wood Mon. Not. R. Astron. Soc. 240 881 1989 1989MNRAS.240..881K Stars, Ap This file contains magnitudes from nearly 50,000 40 second observations of the rapidly oscillating Ap star HR 1217 obtained during nearly 600 hours of observation at various observatories from 1980 to 1986. Most of the obser- vations were made through Johnson B filters, but some were made through other filters. All data in this file were included in a paper entitled The high- overtone p-mode spectrum of the rapidly oscillating Ap star HR 1217 (HD 24712) by Kurtz et al. (1989) and described in the CDS Inf. Bull. (Kurtz 1989). Much of the information published in Kurtz et al. (1989) had been gathered from previously published literature, and some had been obtained by a team established for that paper. Each record holds one observation with the Heliocentric Julian Date given to 5 decimal accuracy and the magnitude given to 4 decimal accuracy. The observations are grouped so that all observations from a single night from each observatory are listed together.
The data published in Kurtz et al. (1989) included observations previously published as follows: Julian Dates Source of data ------------ -------------- JD2444540-2444643 Kurtz (1982) JD2444849-2444953 Kurtz & Seeman (1983) JD2445661-2445664 H. J. Wood (unpublished) JD2445690-2445693 Kurtz, Schneider & Weiss (1985) JD2446712-2446784 original (Kurtz et al. 1989)
Data filter Code for filter used There are amplitude variations from filter to filter and possibly phase shifts, too. Data from different filters should not be mixed unknowingly. JB = Johnson B (most observations were taken with this filter) JV = Johnson V SU = Stromgren u SV = Stromgren v, etc. --- obs Code for observatory CTIO = Cerro Tololo Inter-American Observatory ESO = European Southern Observatory LO = Lowell Observatory MDO = McDonald Observatory MKO = Mauna Kea Observatory MSSSO = mount Stromlo and Siding Spring Observatory MJO = Mount John Observatory SAAO = South African Astronomical Observatory WO = The Florence and George Wise Observatory --- JD Full Julian date of individual observation d mag Magnitude mag Julie Anne Watko SSDOO/ADC 1996 May 22 II_146.xml Catalogue of Diffuse Interstellar Band Measurements 2149 II/149 Diffuse Interstellar Band Measurements Catalogue of Diffuse Interstellar Band Measurements T P Snow Jr. D G York D E Welty Astron. J. 82 113 1977 1977AJ.....82..113S II/135 : Supplement to the Catalog of DIB (Guarinos, 1988) Baerentzen, Gammelgaard, Hilberg, Jorgenson, Kristenson, Nissen, and Rudkjobing (1967) J. Obs. 50, 83. Beals and Blanchet (1938) M.N.R.A.S. 98, 398. Blanco, Demers, Douglas, and Fitzgerald (1968) Pub. U.S. Naval Obs. 21, 1. Bromage and Nandy (1973) A.A. 26, 17. Butler and Seddon (1958a) Publ. R. Obs. Edin. 2, 113. Butler and Seddon (1958b) Publ. R. Obs. Edin. 2, 187. Duke (1951) Ap. J. 113, 100. Gammerlgaard (1975) A.A. 43, 85. Greenstein and Aller (1950) Ap.J. 111, 328. Herbig (1975) Ap.J. 196, 129. Hiltner (1956) Ap.J.Suppl. 2, 389. Kennedy and Buscombe (1974) MK, Spectral Classifications Published Since Jaschek's La Plata Catalogue (Northwestern U., Evanston, IL). Marionni (1971) Unpublished. Merrill, Sanford, Wilson, and Burwell (1937) Ap.J. 86, 274. Murdin (1972) M.N.R.A.S. 157, 461. Serkowski, Mathewson, and Ford (1975) Ap.J. 196, 261. Snow (1973) A.J. 78, 913. Snow, York, and Welty (1977) A.J. 82, 113. Stoeckly and Dressler (1964) Ap.J. 139, 240. Underhill (1956) Publ. DAO 10, 201. Walker (1963) M.N.R.A.S. 125, 141. Walker and Hodge (1966) Publ. DAO 12, 401. Wampler (1966) Ap.J. 144, 921. Wu (1972) Ap.J. 178, 681. Interstellar medium Spectroscopy This catalog contains diffuse band data collected from an exhaustive search of the literature and reduced to a common measurement system. The authors have adopted Herbig (1975ApJ...196..129H) as a standard data set for DIB measurements.
Diffuse band data (Table III(b) of paper) Name Designation of the star --- GLON Galactic longitude number=4 be aware that some positions (especially those with Ref1=24 from Gammelgaard, 1975A&A....43...85G) are only accurate to 0.1deg! The * in the Note column indicates that the position is missing in the published table, and was added in February 1997 with the help of the SIMBAD data-base. There are however 3 stars with missing positions, all from Walker (1963MNRAS.125..141W): Arp e and Arp b (designated as "Special Cases" SC 900002 and SC 900003 in the published table), and BD+61 2615 (which does not exist in Bonner Durchmusterung) deg GLAT Galactic latitude number=4 be aware that some positions (especially those with Ref1=24 from Gammelgaard, 1975A&A....43...85G) are only accurate to 0.1deg! The * in the Note column indicates that the position is missing in the published table, and was added in February 1997 with the help of the SIMBAD data-base. There are however 3 stars with missing positions, all from Walker (1963MNRAS.125..141W): Arp e and Arp b (designated as "Special Cases" SC 900002 and SC 900003 in the published table), and BD+61 2615 (which does not exist in Bonner Durchmusterung) deg Note '*' See Note number=4 be aware that some positions (especially those with Ref1=24 from Gammelgaard, 1975A&A....43...85G) are only accurate to 0.1deg! The * in the Note column indicates that the position is missing in the published table, and was added in February 1997 with the help of the SIMBAD data-base. There are however 3 stars with missing positions, all from Walker (1963MNRAS.125..141W): Arp e and Arp b (designated as "Special Cases" SC 900002 and SC 900003 in the published table), and BD+61 2615 (which does not exist in Bonner Durchmusterung) --- Ac4430 Central depth of the continuum at 4430 A number=1 These measurements have been converted statistically to a common measurement system by the authors, adopting the data of Herbig (1975ApJ...196..129H) as the standard data set, and using a least-squares fitting method. % W5780 Equivalent width (in A) of 5780 A line number=1 These measurements have been converted statistically to a common measurement system by the authors, adopting the data of Herbig (1975ApJ...196..129H) as the standard data set, and using a least-squares fitting method. 0.1nm W5797 Equivalent width (in A) of 5797 A line number=1 These measurements have been converted statistically to a common measurement system by the authors, adopting the data of Herbig (1975ApJ...196..129H) as the standard data set, and using a least-squares fitting method. 0.1nm W6284 Equivalent width (in A) of 6284 A line number=1 These measurements have been converted statistically to a common measurement system by the authors, adopting the data of Herbig (1975ApJ...196..129H) as the standard data set, and using a least-squares fitting method. 0.1nm E(B-V) Colour excess in the UBV system mag lambda Wavelength, given in microns, at which the polarization is maximum um MaxPol Maximum value of the polarization number=2 These polarization data are primarily from Hiltner (1956ApJS....2..389H) or Serkowski et al. (1975ApJ...196..261S) or from the several references given in the latter paper. % Vmag Magnitude mag SpType MK spectral type --- Ref1 Reference for position, photometry and spectroscopy number=3 The references below 100 indicate the diffuse band reference (from table II of paper): 1. Murdin (1972MNRAS.157..461M) 3. Snow (1973AJ.....78..913S) 4. Wu (1972ApJ...178..681W) 5. Duke (1951ApJ...113..100D) 6. Walker (1963MNRAS.125..141W) (first system) 7. Walker (1963MNRAS.125..141W) (second system) 8. Merrill et al (1937ApJ....86..274M) 9. Underhill (1956PDAO...10..201U) 10. Stoeckly and Dressler (1964ApJ...139..240S) 11. Wampler (1966ApJ...144..921W) 12. Walker and Hodge (1965PDAO...12..401W) 14. Bromage and Nandy (1973A&A....26...17B) 15. Marionni (1971, unpublished) 17. Butler and Seddon (1958PROE....2..113B) 18. Butler and Seddon (1960PROE....2..187B) 21. Greenstein and Aller (1950ApJ...111..328G) 22. Beals and Blanchet (1938MNRAS..98..398B) 23. Baerentzen et al (1967JO.....50...83B) 24. Gammelgaard (1975A&A....43...85G) 30. Herbig (1975ApJ...196..129H) The references above 100 indicate other general catalogues, eventually combined with a diffuse band reference: 100-130 Catalogue of Kennedy and Buscombe (1974; see Cat. <III/78>), plus the diffuse band reference corresponding to the last two digits. 200-230 Blanco et al (1968 ; see Cat. <II/4>) plus the corresponding diffuse band reference 300-330 Hiltner (1956ApJS....2..389H) plus the corresponding diffuse band reference 400-430 Bonner Durchmusterung (Cat. <I/122> and <I/119>), or Cordoba Durchmusterung (Cat. <I/114>), plus the corresponding diffuse band reference --- RefIDB Reference for Interstellar Data number=3 The references below 100 indicate the diffuse band reference (from table II of paper): 1. Murdin (1972MNRAS.157..461M) 3. Snow (1973AJ.....78..913S) 4. Wu (1972ApJ...178..681W) 5. Duke (1951ApJ...113..100D) 6. Walker (1963MNRAS.125..141W) (first system) 7. Walker (1963MNRAS.125..141W) (second system) 8. Merrill et al (1937ApJ....86..274M) 9. Underhill (1956PDAO...10..201U) 10. Stoeckly and Dressler (1964ApJ...139..240S) 11. Wampler (1966ApJ...144..921W) 12. Walker and Hodge (1965PDAO...12..401W) 14. Bromage and Nandy (1973A&A....26...17B) 15. Marionni (1971, unpublished) 17. Butler and Seddon (1958PROE....2..113B) 18. Butler and Seddon (1960PROE....2..187B) 21. Greenstein and Aller (1950ApJ...111..328G) 22. Beals and Blanchet (1938MNRAS..98..398B) 23. Baerentzen et al (1967JO.....50...83B) 24. Gammelgaard (1975A&A....43...85G) 30. Herbig (1975ApJ...196..129H) The references above 100 indicate other general catalogues, eventually combined with a diffuse band reference: 100-130 Catalogue of Kennedy and Buscombe (1974; see Cat. <III/78>), plus the diffuse band reference corresponding to the last two digits. 200-230 Blanco et al (1968 ; see Cat. <II/4>) plus the corresponding diffuse band reference 300-330 Hiltner (1956ApJS....2..389H) plus the corresponding diffuse band reference 400-430 Bonner Durchmusterung (Cat. <I/122> and <I/119>), or Cordoba Durchmusterung (Cat. <I/114>), plus the corresponding diffuse band reference --- Francois Ochsenbein CDS 1997 Feb 27 CDS would like to thank Mme F. Boisselier for the typing of the machine readable version of the catalogue. UNKNOWN UNKNOWN * The catalogue was keypunched at CDS under the control of J. Guarinos. in 1988. * The description was added by Julie Anne Watko [ADC] in June 1996. * The "catalog" file was recreated and checked in February 1997 at CDS (Francois Ochsenbein). Some missing positions were added (stars flagged in column Note, byte 30); a few misalignments were corrected. The blank positions, magnitudes and spectral types in consecutive records dealing with the same star were also filled. II_149.xml A Catalogue of Parameters for Eclipsing Binaries 2150A II/150A Parameters of eclipsing binaries A Catalogue of Parameters for Eclipsing Binaries H K Brancewicz T Z Dworak Acta Astronomica 30 501 1980 1980AcA....30..501B II/139 : General Catalog of Variable Stars (GCVS), 4th Ed. (Kholopov+ 1988) V/46 : Classical (Evolved) Algol-Type Binary Candidates (Budding 1984) Cester B., et al.: 1979, Mem. Soc. Astron. Ital., 50, 551 =1979MmSAI..50..551C Cester B., et al.: 1980, Mem. Soc. Astron. Ital., 51, 197 =1980MmSAI..51..197C Koch, R.H., Plavec, M. and Wood, F.B.: 1970, "A catalogue of Graded Photometric studies of Close Binaries", Publ. Univ. Penn. Astr. Series, Volume X, Philadelphia Svechnikov, M.A.: 1969, Katalog orbitalnyich elementov, mass i svetimostei tesnyich dvoinyich zvezd, A.M.Gorky University of the Urals, Sverdlovsk. Binaries, eclipsing An iterative method has been used to compute the geometric and physical parameters of 1048 eclipsing binary stars.
The catalogue Name Name of star --- Cester * if the star is present in Cester's (1979, 1980) catalogue & first supplement --- Per Period in days d Plx Parallax 10-5arcsec Sep Separation between the components in Solar radii solRad R1 Radius of brighter component solRad R2 Radius of fainter component solRad RL1 Percent of filling up of Roche-lobe % RL2 Percent of filling up of Roche-lobe % L1 Absolute bolometric luminosity solLum L2 Absolute bolometric luminosity solLum T1 Effective temperature K T2 Effective temperature K M Sum of masses in solar units solMass q Mass ratio q = M2/M1 --- M1 Mass of brighter component (solar masses) solMass Class Traditional Classification from GCVS (Kukarkin et al, cat. <II/139>) See GCVS (cat. <II/139>), principal classes are: A = Algol type E = Eclipsing binary B = beta Lyr type W = W UMa type --- Kopal Kopal's geometrical classification this class depends on Roche-lobe radii, as: C = Contact system (ex. W UMa) D = Detached system (ex. beta Lyr) S = Semi-detached system (ex. Algol = beta Per) --- Sp Spectrum The colon denotes uncertain information, round brackets denote that the adopted spectrum for a fainter component was taken from Koch et al. (1970), and square brackets that the adopted spectrum was taken from Svechnikov (1969) --- Joseph Florsch , Francois Ochsenbein CDS 1996 Jun 21 UNKNOWN UNKNOWN * The catalogue was keystroked at CDS in 1987 from the published table, which is of poor quality * 21-Jun-1996 (version A): following remarks by Eric Lefevre <Eric.Lefevre@obspm.fr>, a consistency check of the masses was performed and led to corrections to the following 14 stars: LR ARA RX ARI ZZ AUR AK AUR UZ CMI UW CAP V402 CEN NY CEP V388 CYG BO HER LX PER AW UMA RV VEL TT VEL * 29-Jun-1999: corrected NU SGR into UPS SGR (F. Ochsenbein) II_150A.xml New Subdwarfs. IV. UBV Photometry of 1690 High-Proper-Motion Stars 2152 II/152 UBV Photometry of 1690 High-Proper-Motion Subdwarfs New Subdwarfs. IV. UBV Photometry of 1690 High-Proper-Motion Stars A Sandage C T Kowal AJ 91 1140 1986 1986AJ.....91.1140S Photometry, UBV Stars, subdwarf Three-color UBV photometry is given for 1690 high-proper motion stars, providing a finding list for potential high-velocity stars of various metallicity values. The purpose of the survey is to obtain candidates for trigonometric programs on subdwarfs and to enlarge the sample with which to study the relation between stellar kinematics and metal abundance. The observations were made with the 60- and 100-inch Mount Wilson reflectors and the Carnegie 20-inch reflector at Palomar.
The catalog ID Giclas (G), L, misc. identifier --- Comp1 Component designation (A, B) --- DM_ID Prefix for DM identifier (BD, SD) --- DM_No Durchmusterung number --- DM_suff Supplemental DM letter --- Comp2 Component letter designation --- HD Henry Draper (or Extension) number --- RAh R.A. B1950 (hours) h RAm RA B1950 (minutes) min RAs RA B1950 (seconds of time) s DE- Dec. at B1950 (sign) --- DEd Dec. at B1950 (degrees) deg DEm Dec. at B1950 (minutes) arcmin pm Total proper motion (annual) arcsec angle Position angle of proper motion deg V Observed V magnitude mag B-V Observed B-V color mag U-B Observed U-B color mag d(U-B) (U-B)Hyades - (U-B) at (B-V) WD indicates a white dwarf. mag n_obs Number of observations The number of observations and telescope size are missing for G19-11. --- Tel Telescope identifier (20, 60, or 100) There is an error in the telescope size for G73-71. It is given as J0 and not explained. As the error also occurs in the printed volume, it is impossible to correct. --- Nancy G. Roman ADC/SSDOO 1995 Sep 21 UNKNOWN UNKNOWN The original file appeared exactly as in the published paper. To allow easier cross identifications to be made to major catalogs, the HD and DM identifiers were determined and inserted into the catalog. To begin, the G numbers were rewritten in the current uniform format. For the G-numbered stars only, the Lowell proper-motion catalogs were searched by machine and the cross identifications were written to a separate file, which was then edited to isolate the DM numbers. DM numbers that were not in the cross identifier field because of overflow were found in the remarks to the Lowell catalog and inserted manually. For the southern stars listed in Lowell Bulletin No. 164, where many DM numbers are not given, no attempt was made to cross identify automatically. All equatorial coordinates were then precessed to B1855, B1875, and B1900 so that source catalogs could be consulted. All stars still lacking DM numbers and bright enough to suggest DM membership were checked against the BD and SD catalogs and identified there by their precessed coordinates. The DM numbers were then used to search the Henry Draper Catalogue to identify HD and HDE (volume 100) stars. Cross checks were made manually for any stars lacking HD numbers, but bright enough to possibly be in the HD. Using the precessed coordinates, candidates for membership in the second Henry Draper Extension (volume 112) were then selected based on their positions and the sky coverage of the HDE 112 charts. Using appropriate coordinates, the area of each candidate was then found on the correct chart. Final identifications were made using the finding charts for the G-numbered stars published in Lowell Bulletins 102 and 112. This check was to ensure that a star located on an HDE chart by its position was indeed the correct G star. As a final check, G stars cross identified independently by Mermilliod in his catalogs of UBV photometry were checked and all discordances were examined and resolved. The uniform edition of this catalog containing cross identifications to the HD and DM catalogs has been prepared by Wayne H. Warren Jr., Hughes STX Corporation, Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA. The undersigned modified the description somewhat to conform to the current standard form and made several corrections to the format table. She also corrected some errors in the catalog file. She thanks Dr. Warren for the substantial effort he has put into improving this catalog. II_152.xml Catalog of Individual UBV Observations of Stars in the Luminous Stars in the Southern Milky Way (LSS) Catalog 2154 II/154 Individual UBV Observations of LSS Stars Catalog of Individual UBV Observations of Stars in the Luminous Stars in the Southern Milky Way (LSS) Catalog J S Drilling Louisiana State University Obs. ??? ??? 1989 1989 Photometry, UBV Stars, luminous UBV Photometry of Stars from "Luminous Stars in the Southern Milky Way" by J.S. Drilling, Louisiana State University Observatory, 22 July 1989.
UBV measurements LSS LSS number (Stephenson and Sanduleak 1971) --- Comp Component identification if a double star. Where this byte is blank for the same LSS star, both components were included in the diaphragm. --- date Heliocentric Julian date of observation d V V magnitude mag B-V B-V color index mag U-B U-B color index mag Airmass Airmass --- C.-H. Joseph Lyu Hughes STX/NASA and Joseph Florsch CDS 1995 May 25 II_154.xml Catalogue of Apparent Diameters and Absolute Radii of Stars, 2nd Edition 2155 II/155 Apparent Diameters and Absolute Radii of Stars Catalogue of Apparent Diameters and Absolute Radii of Stars, 2nd Edition M Fracassini L E Pasinetti-Fracassini L Pastori R Pironi Bull. Inf. CDS 35 121 1988 1988BICDS..35..121F Stars, diameters For 7255 stars this catalog lists all values of the apparent and absolute radii from the literature. Data were compiled beginning 1950 up to 1985, including some data from 1986 and 1987. The catalogue was ordered by identification by HD number or BD number followed by variables with constellation names in alphabetical order, followed by other abbreviations. The HD and BD numbers were given priority 1 and 2 respectively over the other identifications. Hence variable stars can be found under the name of the constellation only when HD and BD numbers are lacking. The apparent magnitudes and spectral types are those reported by the authors, as they are basic data used in some methods for obtaining the stellar diameters.
catalog data file ID1 HD or BD number or other identification --- ID2 Bayer,Flamsteed or other identification --- mag Apparent visual magnitude mag Sp MK Spectral type --- Diam Apparent stellar diameter in seconds of arc arcsec Rad Absolute radius in solar units solRad Meth Method of determination, see file methods.dat The following Table describes the classification of the methods: DIRECT METHODS ---------------------------------------------------------------------- CODE METHOD REFERENCES -- --------------------- ------------------------------------------- 1 Interferometer of Michelson,A.A.,Pease,F.G.: 1921, Astrophys. Michelson and Pease J. 53, 249. =1921ApJ....53..249M Intensity interfe- Hanbury Brown,R.,Davis,J.,Allen,L.R.,Rome, rometer J.M.: 1967, Monthly Not.Roy.Astron.Soc. 137, 393. =1967MNRAS.137..393B 2 Diffraction - Arnulf,A.: 1936, Compt.Rendus Acad.Sci. Lunar occultations Paris 202, 115. =1936CRA...202..115A Williams,J.D.: 1939, Astrophys.J. 89, 467. =1939ApJ....89..467W 3A Star scintillation - Tichov,G.: 1921, Mitt.Leshafts Color changes Inst.Lenigrad 2, 126. 3B Star scintillation - Gezari,D.Y.,Labeyrie,A.,Stachnik,R.V.: Image changes:speckle 1972, Astrophys.J. 173, L1. interferometry =1972ApJ...173L...1G 4 Eclipsing and spec- Russell,H.N.: 1911, Astrophys.J. 35, 315. troscopic binaries Lehman-Filh?s,R.: 1894, Astron.Nach. 130, 17. 5 Pulsating stars Van Hoof,A.: 1945, Publ.Lab.Astron.Geodes. Univ.Louvain XI, No.100. 5A Pulsating stars Wesselink,A.J.: 1946, Bull.Inst. Netherlands X, 91. =1946BAN....10...91W 5B Pulsating stars Balona,L.A.: 1977, Monthly Not.Roy.Astron. Soc. 178, 231. =1976MNRAS.178..231 5C Pulsating stars Methods which can not be included in the groups 5, 5A and 5B -- --------------------- ------------------------------------------- INDIRECT METHODS -- --------------------- ------------------------------------------- 6A Intrinsic brightness Pickering,E.C.: 1880, Proc.Amer.Acad.Arts and color and Sciences 16, 1. 6B " " Russell,H.N.: 1920, Publ.Astron.Soc.Pacific 32, 307. =1920PASP...32..307R 6C " " Hertzsprung,E.: 1922, Ann.Leiden XIV, 1. =1922AnLei..14....1H 6D " " Pettit,E.,Nicholson,S.: 1928, Astrophys.J. 68, 279. =1928ApJ....68..279P 6E " " Chalonge,D.,Divan,L.: 1950, Compt.Rendus Acad.Sci. Paris 231, 331. =1950CRA...231..331C 6F " " Fracassini,M.,Pasinetti,L.E.: 1967, Atti XI Riunione Soc.Astron.It. Padova. Fracassini,M.,Gilardoni,G.,Pasinetti,L.E.: 1973, Astrophys.Space Sci. 22, 141. =1973Ap&SS..22..131F 6G " " Gray,D.F.: 1967, Astrophys.J. 149, 317. =1967ApJ...149..317G 6H " " Wesselink,A.J.: 1969, Monthly Not.Roy. Astron. Soc. 144, 297. =1969MNRAS.144..297W 6I " " Barnes,T.G.,Evans,D.S.: 1976, Monthly Not. Roy.Astron.Soc. 174, 489 =1976MNRAS.174..489B 6K " " Leone,S.: 1978, Atti Acc.Scienze, Lettere ed Arti di Palermo Ser. IV, 35, 21. 6L " " Walker,H.J., Schonberner,D.: 1981, Astron. Astrophys. 97, 291. =1981A&A....97..291W -- --------------------- ------------------------------------------- Codes for bibliographic references: The following codes for the bibliographic references are used: --------- ----------------------------------------------------------- EG/GR Eggen,O.J.,Greenstein,J.L.: 1965a, =1965ApJ...141...83E Eggen,O.J.,Greenstein,J.L.: 1965b, =1965ApJ...142..925E Eggen,O.J.,Greenstein,J.L.: 1967, =1967ApJ...150..927E Greenstein,J.L.: 1969, =1969ApJ...158..281G Greenstein,J.L.: 1970, =1970ApJ...162L..55G Greenstein,J.L.: 1974, =1974ApJ...189L.131G Greenstein,J.L.: 1975, =1975ApJ...196L.117G G Giclas,H.L.,Burnham,R.,Thomas,N.G.: Lowell proper motions I to XV, Lowell Obs.Bull., 1960 to 1970, No.89, 102, 112, 120, 122,124, 129, 136, 140, 144, 150, 151, 152. (Catalog <I/79>) Giclas,H.L.,Burnham,R.,Thomas,N.G.: A list of white dwarfs suspects I, II, III, Lowell Obs.Bull., 1965 to 1970, No.125, 141, 153. GLIESE Gliese,W.: 1969, Veroeff.Astron.Rech.Inst. Heidelberg 22. (Catalog <V/35>) IRC Neugebauer,G.,Leighton,R.B.: 1969, Two-micron sky survey, California Inst.Tech., NASA SP-3047. (Catalog <II/2>) LDS 157 C Luyten,W.J.: 1952, Astrophys.J. 116, 283. =1952ApJ...116..283L STOCK Stock.J.: 1956, Astrophys.J. 123, 258. =1956ApJ...123..253S Stock,J.,Wroblewski,H.: 1972, Publ.Dept.Astron.Univ.Chile, Obs.Astron.Nac. Vol.II, No.3, 59. =1972PDAUC...2...59S Stock,J.,Osborn,W.,Ibanez,M.: 1976, Astron.Astrophys.Suppl.Ser. 24, 35. =1976A&AS...24...35S V McCook,G.P.,Sion,E.M.: 1977, Villanova Univ.Obs.Contr. No.2. (Catalog <III/129>) V 78 Martin,W.C.: 1938, Ann.Sterrewacht Leiden 17, part 2 (star in Omega Cen). =1938AnLei..17b...1M WD McCook,G.P.,Sion,E.M.: 1977, Villanova Univ.Obs.Contr. No.2. (Catalog <III/129>) Liebert,J.,Stockman,H.S.: 1980, Publ.Astron.Soc.Pacific 92, 657. =1980PASP...92..657L WOOLLEY Woolley,R.,Epps.E.A.,Penston,M.J.,Pocock,S.B.: 1970, Publ.Annals Roy.Obs.Greenwich 5,1. (Catalog <V/32>) WORLEY A catalogue of visual binary orbits, Publ. U.S. Naval Obs., Second Ser. Vol.XVIII Part III, Washington 1963. (Catalog <V/39>) --------- ----------------------------------------------------------- --- ref key to reference, see file refs.dat --- rem Remarks, see file remarks.dat --- PRDiam printed value Apparent stellar diameter arcsec PRRad printed value stellar radius solRad references to the catalog ref key to reference --- --- separator --- reftext the reference --- remarks to the catalog Nrec number of records in this key (0=extension record) --- ID source identification --- rem key to remark --- text remark text The following symbols have been used: symbol meaning ------ ------------------------------- Ro = solar radius ? = micron l = wavelength ? = angular diameter ?ud = uniform disk angular diameter ?ld = limb-darkening angular diameter dl = delta lambda ------ ------------------------------- --- N.P.M. Kuin ADC 1994 Nov 16 UNKNOWN UNKNOWN * 01-Sep-1998: radius of star HD 180939 corrected in file cadars.dat II_155.xml IRAS Faint Source Catalog, |b| > 10 Degrees, Version 2.0 2156A II/156A IRAS Faint Source Catalog, |b| > 10, Version 2.0 IRAS Faint Source Catalog, |b| > 10 Degrees, Version 2.0 M Moshir G Copan T Conrow H McCallon P Hacking D Gregorich G Rohrbach M Melnyk W Rice L Fullmer T J Chester Infrared Processing and Analysis Center ??? ??? 1989 1989ifss.book.....M II/125 : IRAS Point Source Catalog II/126 : IRAS Serendipitous Survey Catalog II/174 : IRAS 2Jy Redshift Survey Data File II/190 : IRAS Minor Planet Survey Data Base VII/73 : IRAS Small Scale Structure Catalog VII/91 : IRAS Asteroid and Comet Survey VII/109 : IRAS Observations of Large Optical Galaxies VII/113 : Catalogued Galaxies + QSOs observed in IRAS Survey Infrared sources Photometry, infrared Surveys The Faint Source Survey (FSS) is the definitive Infrared Astronomical Satellite data set for faint point sources. The FSS was produced by point-source filtering the individual detector data streams and then coadding those data streams using a trimmed-average algorithm. The resulting images, or plates, give the best estimate from the IRAS survey data of the point source flux density at every surveyed point of the sky. The Faint Source Catalog (FSC) is a compilation of the sources extracted from the FSS plates that have met reasonable reliability requirements. Averaged over the whole catalog, the FSC is at least 98.5% reliable at 12 and 25 microns, and ~94% at 60 microns. For comparison, the IRAS Point Source Catalog (PSC) is >99.997% reliable, but the sensitivity of the FSC exceeds that of the PSC by about a factor of 2.5. The FSC contains data for 173,044 point sources in unconfused regions with flux densities typically above 0.2 Jy at 12, 25, and 60 microns, and above 1.0 Jy at 100 microns. The FSS plates are somewhat more sensitive but less reliable than the FSC; typically, only sources with SNR > 5 - 6 in the plates are contained in the FSC. Sources with SNR > 3 but which do not meet the reliability requirements of the FSC are catalogued in the Faint Source Reject File (FSR). The data products, the processing methods used to produce them, results of an analysis of these products, and cautionary notes are given in the Explanatory Supplement to the IRAS Faint Source Survey (see references in fsc.doc).
IRAS Faint Sources Name Source name --- RAh Hours RA, equinox 1950.0, epoch 1983.5 h RAm Minutes RA, equinox 1950.0, epoch 1983.5 min RAds Deci-seconds RA 0.1s DE- Sign of DEC, equinox 1950.0, epoch 1983.5 --- DEd Degrees Dec, equinox 1950.0, epoch 1983.5 deg DEm Minutes Dec, equinox 1950.0, epoch 1983.5 arcmin DEs Seconds Dec, equinox 1950.0, epoch 1983.5 arcsec UncMajor Uncertainty ellipse major axis arcsec UncMinor Uncertainty ellipse minor axis arcsec PosAng Uncertainty ellipse position angle deg Nobs_12 Number of times observed at 12um --- Nobs_25 Number of times observed at 25um --- Nobs_60 Number of times observed at 60um --- Nobs_100 Number of times observed at 100um --- Fnu_12 Non-color corrected flux density at 12um Jy Fnu_25 Non-color corrected flux density at 25um Jy Fnu_60 Non-color corrected flux density at 60um Jy Fnu_100 Non-color corrected flux density at 100um Jy FQual_12 Flux density quality at 12um --- FQual_25 Flux density quality at 25um --- FQual_60 Flux density quality at 60um --- FQual_100 Flux density quality at 100um --- Relunc_12 Percent relative flux density uncertainty at 12um --- Relunc_25 Percent relative flux density uncertainty at 25um --- Relunc_60 Percent relative flux density uncertainty at 60um --- Relunc_100 Percent relative flux density uncertainty at 100um --- MinRel Percent minimum source reliability --- SNR_12 SNR at 12um --- SNR_25 SNR at 25um --- SNR_60 SNR at 60um --- SNR_100 SNR at 100um --- LocSNR_12 Local SNR at 12um --- LocSNR_25 Local SNR at 25um --- LocSNR_60 Local SNR at 60um --- LocSNR_100 Local SNR at 100um --- Area_12 Number of pixels above threshold at 12um --- Area_25 Number of pixels above threshold at 25um --- Area_60 Number of pixels above threshold at 60um --- Area_100 Number of pixels above threshold at 100um --- CatNbr Number of nearby catalog sources --- ExtNbr_12 Number of nearby extractions at 12 um --- ExtNbr_25 Number of nearby extractions at 25 um --- ExtNbr_60 Number of nearby extractions at 60 um --- ExtNbr_100 Number of nearby extractions at 100 um --- Cirrus Number of nearby 100 um-only extractions --- Confuse Confusion flag, 1 per band, hex-encoded --- NoisCor_12 Noise correction factor at 12um --- NoisCor_25 Noise correction factor at 25um --- NoisCor_60 Noise correction factor at 60um --- NoisCor_100 Noise correction factor at 100um --- NID Number of positional associations --- IDType Type of object --- NoisRat_12 Ratio of 85% to 68% of flux distribution at 12um --- NoisRat_25 Ratio of 85% to 68% of flux distribution at 25um --- NoisRat_60 Ratio of 85% to 68% of flux distribution at 60um --- NoisRat_100 Ratio of 85% to 68% of flux distribution at 100um --- Associations Name IRAS source name --- RecNo Main data table record number for IRAS source --- CatNo Catalog number number=1 Detailed explanations are presented in the file meaning.txt. --- Source Source identification --- Type Source type or spectral class --- Radius Radius vector from IRAS source to association arcsec Pos Position angle from IRAS source to association deg DstMajor Distance from IRAS source to association arcsec DstMinor Distance from IRAS source to association arcsec Field1 Object data field 1, catalog dependent --- Field2 Object data field 2, catalog dependent --- Field3 Object data field 3, catalog dependent --- fsc.doc CD-ROM Documentation meaning.txt Details of association catalogues CDS 1993 Feb 24 II_156A.xml Catalogue of Photoelectric Photometry in the Vilnius system 2157A II/157A Photoelectric Photometry in Vilnius system Catalogue of Photoelectric Photometry in the Vilnius system V Straizys A Kazlauskas E Jodinskiene A Bartkevicius Institute of Physic Lithuanian Academy of Science, The Astronomical Observatory of the Vilnius State University ??? ??? 1989 Photometry, Vilnius This catalogue contains the results of photoelectric photometry of 4849 stars in the Vilnius seven-color photometric system UPXYZVS obtained in 1968-1988. The filters of the Vilnius system are: ------------------- Filter Lambda Width (A) (A) ------------------- U 3450 400 P 3740 260 X 4050 220 Y 4660 260 Z 5160 210 V 5440 260 S 6550 200 -------------------
The catalogue of Vilnius Photometry LID Code-number in the Lausanne/Geneva system number=1 see file "refs", Table 3. This designation includes the components of double or multiple stars (A, B, AB etc) in bytes 13-14 --- DM Durchmusterung (BD/CD/CPD) numbers. --- Name Bayer or GCVS (variable) name of star. --- VarFlag 'VAR' - for variable star included in GCVS, 'VAR?' for stars suspected of variability. --- VarType Type of Variability taken from GCVS. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s u_RAs ':' if precision of equatorial coordinates is less than 1s. --- DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Vmag The magnitude V. mag u_Vmag ':' if precision of Vmag less than 0.03 mag., 'V' for variable --- r_Vmag Source of V magnitude number=2 Source of Vmag is coded as follows: blank - if V is measured in the Vilnius-system, 'N' - if V is taken from the catalogue of B. Nicolet (1978) =1978A&AS...34....1N 'M' - if V is taken from the UBV Photoelectric Photometry Catalogue of J.C. Mermilliod (1986) (CDS Catalogue: II/122B) =1987A&AS...71..413M 'L' - if V is taken from other UBV sources. --- U-P U-P photometric index mag u_U-P Uncertainty flag (:) on U-P --- P-X P-X photometric index mag u_P-X Uncertainty flag (:) on P-X --- X-Y X-Y photometric index mag u_X-Y Uncertainty flag (:) on X-Y --- Y-Z Y-Z photometric index mag u_Y-Z Uncertainty flag (:) on Y-Z --- Z-V Z-V photometric index mag u_Z-V Uncertainty flag (:) on Z-V --- V-S V-S photometric index mag u_V-S Uncertainty flag (:) on V-S --- Nobs Number of measurements. --- STD 'S' for Standard star --- r_SpType Source of spectral classification number=3 Source of the spectral classification is as follows: blank - from the Vilnius photometric system, 'J' - from M.Jaschek Catalogue of Selected Spectral Types in the MK system (CDS Catalogue: III/42) =1978BICDS..15..121J 'K' - from P.M.Kennedy MK Classification Extension Catalogue (Mount Stromlo, Australia, ed. 1978) 'L' - from other sources. The preference is given to M.Jaschek catalogue if the same star has different spectral classifications in references. Exception is made for the Bright Star Catalogue, GCVS and General Catalogue of Cool Carbon Stars of C.B. Stephenson (Publ. Warner and Swasey Obs., Vol. 1, No. 4, 1973). In such cases the spectral classification is taken from these catalogues and are marked 'L'. --- SpType Spectral classification number=4 in addition to normal spectral classes O, B, A, F, G, K, M and luminosity classes Ia, Ib, Iab, II, III, IV, V, the following designations are used: R,N,C - Carbon stars, S - Zirconium stars, CN - Cyanogen stars, WR, WC, WN - Wolf-Rayet stars, DO, DB, DA, DZ, DQ - White dwarfs of different types. The next designations are added to main spectral classification to mark some peculiarities in spectrum: P - peculiarity in spectrum, E - emission in spectrum, M - metallic-line star, N - spectral lines widened by axial rotation, S - narrow spectral lines, BA - Barium stars, CH - stars with strong G-band, MD - metal-deficient star, NN - very wide spectral lines, OF - emission-line O-type star, SB - spectroscopic binary star, SD - subdwarf (dwarf with large metal-deficiency) WG - stars with weak G-band, BHB - blue horizontal branch star, RHB - red horizontal branch star, MDE - extreme metal-deficient star, MDG - metal-deficient giant, MDGE - extreme metal-deficient giant, MDSG - metal-deficient subgiant, MDSGE - extreme metal-deficient subgiant, SHELL,SH - shell-star. The absence of spectral classification means that either no spectral classification is known for given star, or the star is impossible to classify photometrically. --- Ref Reference for measurement in the Vilnius photometric system (see file "refs", Table 2) --- Francois Ochsenbein CDS 1995 Oct 02 UNKNOWN UNKNOWN * December 1989: tape received at CDS from Moscow Astronomical Data Centre * 02-Oct-1995: description standardized at CDS; a few errors have been detected and corrected: - 'null' characters converted to blanks - the "ST" (standard stars) initially in bytes 111-112 moved to byte 113 - the missing decimal points in DEm column have been added - a "/" character appearing in byte 71 of record #1629 (1.00090068) changed to a blank - a ":" character appearing in byte 80 of record #4593 (6.20205021) changed to a blank II_157A.xml Theoretical Colours and Isochrones for some Hubble Space Telescope Colour Systems 2160 II/160 HST Colour System Isochrones Theoretical Colours and Isochrones for some Hubble Space Telescope Colour Systems B Edvardsson R A Bell MNRAS 238 1121 1989 1989MNRAS.238.1121E Colors Isochrones Photometry, surface This dataset contains two related data types. The first (1 file) is a grid of synthetic surface brightness magnitudes for 21 of the Hubble Space Telescope Wide Field Camera (WFC) pass bands. The magnitudes are calculated from a new set of synthetic spectra for effective temperatures in the range 4000 to 7250 K, surface gravities typical of dwarfs and sub-giants, and for metallicities in the range solar to one-thousandth solar (280 synthetic spectra). The second is the absolute magnitudes for each of the 21 pass bands for a set of globular cluster isochrones with different helium abundances, metallicities, oxygen abundances and ages. The isochrones were taken from VandenBerg and Bell (1985), Bell and VandenBerg (1987), Hesser et al. (1987) and McClure et al. (1987) all of whom originally published them for the Cousins VRI, Johnson UBV, Stromgren and Thuan-Gunn photometric systems.
Surface Brightness Mags for grid model spectra Teff Effective Temperature K log_g Logarithmic Surface Gravity (cgs) cm/s2 A/H Logarithmic Metallicity Relative to Sun --- V Johnson V Magnitude The Johnson V and the 21 WFC magnitudes have been normalized to 0 for a model which represents Vega mag 336W WFC Magnitude at 3360A mag 368M WFC Magnitude at 3680A mag 413M WFC Magnitude at 4130A mag 439W WFC Magnitude at 4390A mag 492M WFC Magnitude at 4920A mag 547M WFC Magnitude at 5470A mag 555W WFC Magnitude at 5550A mag 569W WFC Magnitude at 5690A mag 606W WFC Magnitude at 6060A mag 622W WFC Magnitude at 6220A mag 648M WFC Magnitude at 6480A mag 675W WFC Magnitude at 6750A mag 702W WFC Magnitude at 7020A mag 718M WFC Magnitude at 7180A mag 725LP WFC Magnitude at 7250A mag 785LP WFC Magnitude at 7850A mag 791W WFC Magnitude at 7910A mag 814W WFC Magnitude at 8140A mag 850LP WFC Magnitude at 8500A mag 875M WFC Magnitude at 8750A mag 1042M WFC Magnitude at 10420A mag Absolute Mags for Isochrone 1 Absolute Mags for Isochrone 2 Absolute Mags for Isochrone 3 Absolute Mags for Isochrone 4 Absolute Mags for Isochrone 5 Absolute Mags for Isochrone 6 Absolute Mags for Isochrone 7 Absolute Mags for Isochrone 8 Absolute Mags for Isochrone 9 Absolute Mags for Isochrone 10 Absolute Mags for Isochrone 11 Absolute Mags for Isochrone 12 Absolute Mags for Isochrone 13 Age Age Ga Mass Mass solMass Mbol Bolometric Magnitude mag Teff Effective Temperature K log_g Logarithm of Surface g in cm/s2 cm/s2 Mv Johnson Mv Johnson Mv, based on the filter pass-band of Matthews & Sandage (1963) mag 336W Magnitude at 3360A The next 21 columns are magnitudes interpolated from tbl2.dat mag 368M Magnitude at 3680A mag 413M Magnitude at 4130A mag 439W Magnitude at 4390A mag 429M Magnitude at 4290A mag 547M Magnitude at 5470A mag 555W Magnitude at 5550A mag 569W Magnitude at 5690A mag 606W Magnitude at 6060A mag 622W Magnitude at 6220A mag 648M Magnitude at 6480A mag 675W Magnitude at 6750A mag 702W Magnitude at 7020A mag 718M Magnitude at 7180A mag 725LP Magnitude at 7250A mag 785LP Magnitude at 7850A mag 791W Magnitude at 7910A mag 814W Magnitude at 8140A mag 850LP Magnitude at 8500A mag 875M Magnitude at 8750A mag 1042M Magnitude at 10420A mag rem Remark An asterisk (*) signifies that the colours have been extrapolated from the grid. --- Julie Anne Watko SSDOO/ADC 1995 DEec 12 II_160.xml Equatorial Infrared Catalog 2161 II/161 Equatorial Infrared Catalog Equatorial Infrared Catalog L H Sweeney T Richardson Space Applications Corporation ??? ??? 1990 1990 II/2 : Two Micron Sky Syrvey (TMSS) (Neugebauer+ 1969) II/94 : Revised AFGL Sky Survey Catalog and Supplement (Price+ 1983) Photometry, infrared EIC (Equatorial Infrared Catalog) lists positions and other information for 7,220 infrared stars. Each star is described by a 175-byte print record. The fields within each star record are defined here. The catalog was prepared as a result of additional processing of USAF satellite data at 2.7 micrometers for sources within 10 degrees of the celestial equator. Every source has been observed on two or more days or on the same day at times 20 minutes apart. The catalog includes right ascension and declination (equinox B1950.0), flux densities and their standard deviations, galactic coordinates, spectral types, and cross identifications to the numbering systems of EIC-1, the SAO and AFGL catalogs, and the Durchmusterung catalogs.
Catalog data Ident star identification number --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (hours) [B1950] h RAm Right ascension (minutes) min RAs Right ascension (seconds) s e_RAs Standard deviation for RA s DE- Declination sign --- DEd Declination (degrees) [B1950] deg DEm Declination (minutes) arcmin DEs Declination (seconds) arcsec e_DEs Standard deviation for DE arcsec FIR Flux density in the near infrared (average of the 2.7um representative measurements) 10-16W/cm2/um e_FIR Standard deviation for FIR 10-16W/cm2/um o_FIR Number of observations --- SpType Spectral type obtained from HD, AGK3, or SAO with HD first choice, AGK3 second choice, and SAO otherwise for the nearest star within 12 arc seconds in AGK3 or SAO --- Vmag Visual magnitude Visual magnitude from AGK3 or SAO for the nearest star within 12 arc seconds in AGK3 or SAO mag Imag 0.84 micron magnitude from TMSS 0.84 micron magnitude from TMSS for the nearest star within 90 arc seconds in TMSS mag Kmag 2.2 micron magnitude from TMSS 2.2 micron magnitude from TMSS for the nearest star within 90 arc seconds in TMSS --- m4.2 4.2 micron magnitude from AFGL 4.2 micron magnitude from AFGL for the nearest star within 400 arc seconds in AFGL --- pmRA Proper motion in RA from AGK3 or SAO Proper motion from AGK3 or SAO for the nearest star within 12 arc seconds in AGK3 or SAO 10mas/yr pmDE Proper motion in DE from AGK3 or SAO 10mas/yr eAGK3 Distance EIC-AGK3 great circle arc distance, EIC minus AGK3 (or SAO) for the nearest star within 12 arcsec arcsec eSAO Distance EIC-SAO arcsec eTMSS Distance EIC-TMSS great circle arc distance, EIC minus TMSS, for the nearest star within 90 arcsec arcsec eAFGL Distance EIS-AFGL great circle arc distance, EIC minus AFGL, for the nearest star within 400 arcsec arcsec HD Henry Draper star identification number number obtained using the HD-SAO-DM Cross Index, NASA Technical Memorandum 79564 (1978) by T.A. Nagy and J.M. Mead (Catalog <III/135>) --- BD Bonner Durchmusterung zone and star number from HD or AGK3 --- AGK3 AGK3 designation Astronomische Gesellschaft Katalog 3 star identification zone and star number from ARI (Astronomische Rechen- Institut, Heidelberg) tape from Hamburg, 1975 version (Catalog <I/61>) --- SAO SAO designation Smithsonian Astrophysical Observatory star identification number from Star Catalog: Positions and proper motions of 258,997 stars for the epoch and equinox of 1950.0, Publication of the Smithsonian Institute of Washington D.C., No. 4562, 1966 (catalog <I/131>) --- TMSS Two Micron Sky Survey designation Star identification zone and star number from the Two-Micron Sky Survey, NASA SP-3047, 1969 by G. Neugebauer and R.B. Leighton (catalog <II/2>) --- AFGL Air Force Geophysical Laboratory designation Star identification number from the Four Color Infrared Sky Survey: Catalog of Observations at 4.2, 11.0, 19.8, and 27.4 microns, AFGL-TR-76-0208, Air Force Geophysical Laboratory by S.D. Price and R.G. Walker (Catalog <II/94>) --- Joseph Florsch CDS and C.-H. Joseph Lyu Hughes STX/NASA 1995 May 15 UNKNOWN UNKNOWN * supersedes II/96/ * Original documentation prepared by Lee Sweeney and Terry Richardson Space Applications Corporation 2900 South Center Green Court Boulder, Colorado 80301-5418 (303) 440-3544 Contact (from April 1998) at address: 137 Alpine Way, Boulder, Colorado, USA 303-443-6287 Email: sweeneyent@email.msn.com II_161.xml A scanner CCD search for Cepheids and other variables in Crux and Centaurus. 2162 II/162 CCD search in Crux and Centaurus A scanner CCD search for Cepheids and other variables in Crux and Centaurus. J A R Caldwell M J Keane P L Schechter Astron. J. 101 1763 1991 1991AJ....101.1763C Stars, variable Photometry This catalog contains the results of a photometric survey for variable stars in a 9.4 square degree region along the galactic plane in Crux and Centaurus. A total of 300 308 stars were observed at seven epochs over 42 days; 224 524 of these stars were detected at multiple epochs and were tested for possible variations in brightness that exceed observational error. 2422 stars are identified as variable at a formal confidence level of 99%; 270 of the new variables brighter than I=14.0 are classified as long period variables. A list of 242 likely short period variables with RMS amplitudes >=0.060mag is given. From this list, 37 Cepheid candidates were selected after inspection of their light curves.
The complete list of probable variables Observations with RA = 11 39 40 to 12 15 41 and declination = -63 05 12 to -62 46 46 (1950) Observations with RA = 11 39 40 to 12 15 12 and declination = -62 46 47 to -62 27 26 (1950) Observations with RA = 11 39 40 to 12 14 44 and declination = -62 27 27 to -62 03 11 (1950) Observations with RA = 11 39 40 to 12 14 16 and declination = -62 03 12 to -61 47 46 (1950) Observations with RA = 11 39 39 to 12 13 48 and declination = -61 47 47 to -61 24 46 (1950) Observations with RA = 13 10 14 to 13 46 17 and declination = -63 06 09 to -62 54 03 (1950) Observations with RA = 13 10 15 to 13 45 52 and declination = -62 53 19 to -62 36 32 (1950) Observations with RA = 13 10 15 to 13 45 28 and declination = -62 35 49 to -62 23 27 (1950) image Image number number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. --- no Number of object within the image number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. --- RAh Right Ascension, hours (1950) number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. h RAm Right Ascension, minutes (1950) number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. min RAs Right Ascension, seconds (1950) number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. s DE- Declination sign number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. --- DEd Declination, degrees (1950) number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. deg DEm Declination, minutes (1950) number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. arcmin DEs Declination, seconds (1950) number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. arcsec I Cousins I magnitude number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. mag e_I Formal uncertainty in I Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. mag MJD Mean Julian Day number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. d x X position within the image The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. pix y Y position within the image number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. pix class Object classification 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. --- ID Catalog from which it is drawn This is a sequence number assigned for internal use. The decoding is unavailable. number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. --- num_ID Number in source catalog number= Stars with centroids within 12 pixels of the beginning of the image (which, unfortunately, includes the first stars on the variable star list) may have suffered from a software bug in the data acquisition and may have errors bigger than the formal errors. number= The pixels are not square. They are 0.45" in the x direction and either 3.7" or 1.85" in the y direction. The latter are less frequent and go somewhat fainter than the lower resolution observations. number= 1 = single star 2 = galaxy 3 = one component of a multiple star 4 = an object for which the classification is uncertain 5 = too few pixels to determine classification or for which a position was derived beyond the boundaries of the image or fit subraster 6 = should not be in the catalog 7 = too faint to attempt classification 8 = could not be modeled (too bright or cosmic ray) and has been excised number= This is a sequence number assigned for internal use. The decoding is unavailable. --- High amplitude, short-period variables found in this survey Long-period variables found in this survey Name Variable name --- m_Name Multiplicity index on Name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg Dem Declination 1950 arcmin DEs Declination 1950 arcsec Imag I magnitude mag e_Imag rms uncertainty on Imag mag Notes Notes number=1 1. 1st rank Cepheid candidate. 2. 2nd rank Cepheid candidate. 3. Possible eclipse. 4. Possible LPV. 5. Additional photometry obtained 1990 Feb-Apr. 6. Variable is also identified as an IRAS 12{mu} source, see Table 6 7. Variable is also identified as a carbon star, see Table 7 Note: the remarks in table 5 are in bytes 49-61. --- Variable stars identified with IRAS 12 {mu}m sources Name Variable name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg Dem Declination 1950 arcmin DEs Declination 1950 arcsec Imag I magnitude mag IRAS IRAS source --- Notes Notes number=1 1. Variable was classified as LPV and is also listed in Table 5. 2. Variable was classified as short-period variable and is also listed in Table 4. Likely a long period variable observed near minimum or maximum light. 3. Object is also identified as a carbon star, see Table 7 --- *The ABCS carbon stars detected as variables in this survey ABCS Aaronsom C stars number=1 Aaronsom M. et al., 1989, ApJS 70, 637 --- Name Variable star name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Notes Notes number=2 1. Classified as a LPV, see Table 5. 2. Also identified with an IRAS 12{mu} source, see Table 6. --- Nancy Grace Roman SSDOO/ADC 1996 Apr 30 UNKNOWN UNKNOWN The tables were keypunched at CDS; the data files were provided by Dr. P. L. Schechter. The portion of this document which refers to the tables and the Description were prepared by Simona Mei and Patricia Bauer of the CDS in December 1994. II_162.xml The General Catalogue of Photometric Data 2167 II/167 General Catalogue of Photometric Data The General Catalogue of Photometric Data B Hauck C Nitschelm M Mermilliod J -C Mermilliod Astron. Astrophys. Suppl. Ser. 85 989 1990 1990A&AS...85..989H Photometry This catalogue is an index of photometric data published in the astronomical literature until July 1988, and contains 165994 stars.
Main file. Version: April 1990 LID Lausanne identification code (LID) (see num_sys.doc) --- rem Remarks on duplicity and variability --- RAh Right Ascension (1950) h RAm Right Ascension min RAs Right Ascension s DE- Declination (1950) Note that columns 24-25 are blank when the accuracy of declination is only 1'. --- DEd Declination deg DEm Declination arcmin V Johnson V Magnitude mag key1 Keys of the photometric systems. Explanations of the keys are in the file refs.doc --- num_sys.doc Description of the code numbering system refs.doc keys of the photometric systems and references N. Paul M. Kuin ADC/NSSDC 1995 Aug 03 Author's Note: Please, send your comments and found errors to the authors e.g. at e-mail address: mermia@scsun.unige.ch or mermio@scsun.unige.ch UNKNOWN UNKNOWN This introduction file was modified, and the ref file was added at Centre de Donnees astronomiques de Strasbourg (CDS), November 1991. (cats @ simbad.u-strasbg.fr) 3-Aug-1995 the ReadMe file created from earlier documentation [ADC] Periods were added to col. DEm to comply with the F format. II_167.xml Catalogue of Homogeneous Means in the UBV System 2168 II/168 Homogeneous Means in the UBV System Catalogue of Homogeneous Means in the UBV System J -C Mermilliod Institut d'Astronomie, Universite de Lausanne ??? ??? 1991 1991 Photometry, UBV The present catalog supersedes an earlier edition of Nicolet (1978). It is a collection of weighted mean photoelectric values (V, B-V, U-B) for stars measured in the UBV system. The mean values were computed by combining all individual measurements compiled in the catalog of Mermilliod (1987), except those that were clearly found to be erroneous for some reason or another. Some newer observations compiled since 1987 are also included in the means. The procedure for computing the homogeneous means involved the calculation of normal averages weighted by the number of observations in each list (unity when not published). New weights are assigned based on the deviation of each value from the previous mean, then a new weighted mean is computed. This technique is not as rigorous as that used by Nicolet (comparison of each list with the standard system master list), but the latter cannot often be realized effectively in practice, since many lists do not contain enough stars in common with a standard list. Also, there are now so many references (more than 1500) that it is not feasible to analyze each publication with respect to a standard list. This edition of the catalog contains 92964 stars measured since the introduction of the UBV system in 1953. The data included are star identification in the Geneva coded numbering system, double and variable codes, UBV data and their standard deviations, and number of observations. A second file contains the definition of the coded numbering system. The catalog was prepared at the Institut d'Astronomie de l'Universite de Lausanne in Geneva.
Catalog Data IDnum Lausanne identification number (Mermilliod 1978) The Lausanne identification number is comprised of both the IDnum and comp fields. The "D" in the comp field indicates that more than one component of a multiple system was included in the diaphragm when the observation was made. --- comp Lausanne component (D, 1, 2, ...). --- var Variability (V) code. --- numpub Number of publications (separate lists) contributing observations to the means --- Vmean Mean V magnitude (Precision varies) mag Vsigma Standard deviation for Vmean mag l_Vmean Indicates more than o_Vmean observations --- o_Vmean Number of observations for Vmean STD indicates standard star / indicates number is unknown --- B-Vmean Mean (B-V) color index (Precision varies) mag B-Vsigma Standard deviation for B-Vmean --- l_B-Vmean Indicates more than o_B-Vmean observations --- o_B-Vmean Number of observations for B-Vmean --- U-Bmean Mean (U-B) color index (Precision varies) mag U-Bsigma Standard deviation for U-Bmean mag l_U-Bmean Indicates more than o_U-Bmean observations --- o_U-Bmean Number of observations for U-Bmean --- ubvmeans.doc Author's documentation number.doc Numbering system documentation James E. Gass SSDOO/ADC 1997 Sep 05 II_168.xml Long-term photometry of variables at ESO. I - The first data catalogue (1982-1986) 2170 II/170 Long-term photometry of Variables I. Long-term photometry of variables at ESO. I - The first data catalogue (1982-1986) J Manfroid C Sterken A Bruch M Burger M De Groot H W Duerbeck R Duemmler A Figer T Hageman H Hensberge A Jorissen R Madejsky H Mandel H A Ott A Reitermann R E Schulte-Ladbeck O Stahl H Steenman D vander Linden F J Zickgraf Astron. Astrophys., Suppl. Ser. 87 481 1991 1991A&AS...87..481M Long-term photometry of variables at ESO. I - The first data catalogue (1982-1986) J Manfroid C Sterken A Bruch M Burger M De Groot H W Duerbeck R Duemmler A Figer T Hageman H Hensberge A Jorissen R Madejsky H Mandel H A Ott A Reitermann R E Schulte-Ladbeck O Stahl H Steenman D vander Linden F J Zickgraf ESO Sci. Report 8 ??? ??? 1991 1991ESOSR...8....1M II/188 : Long-Term Photometry of Variables at ESO II (1993) II/200 : Long-Term Photometry of Variables at ESO III (1995) II/202 : Long-Term Photometry of Variables at ESO IV (1995) Photometry, uvby Stars, variable This is the first catalogue of photometric data in the Stroemgren system obtained during the period October 1982 - September 1986. Full description can be found in ESO report SP 8. Since our goal is not absolute (all-sky) photometry, the observations should be used for differential photometry only. The mean values of the r.m.s. deviations of the differential measurements of comparison stars are around (from Table 5 of paper) ------------------------------------ System y b-y m1 c1 ------------------------------------ 1 0.0109 0.0088 0.0133 0.0136 4 0.0068 0.0057 0.0079 0.0118 5 0.0087 0.0070 0.0114 0.0114 6 0.0090 0.0078 0.0126 0.0132 7 0.0071 0.0033 0.0041 0.0065 ------------------------------------
The Observations Name Star Identification number=1 The cross-identifications are explained in "stars1" file. Program stars start with the letter P, and comparison stars with A, B ... The following ten stars are not identified in the "stars" file: B1008 C4001 A5015 B5015 B5017 A6009 B6009 A7004 B7004 C9007 --- HJD Heliocentric Julian Date d Airmass Airmass (sec.z) --- umag magnitude mag vmag magnitude mag bmag magnitude mag ymag magnitude mag T/S Telescope/system code --- R Release code --- The list of stars observed (10 stars missing) Name Star Identification, as in "catalog" --- HD HD designation --- HR HR (Bright Star) designation --- DM Durchmusterung (BD, CoD, CPD) designations --- Name2 Other designation --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Sp Spectral classification --- Francois Ochsenbein CDS 1995 Nov 27 UNKNOWN UNKNOWN * 16-Apr-1992: The catalogue was kindly provided to CDS by J.Manfroid * 27-Nov-1995: ReadMe file revisited at CDS (Francois Ochsenbein) II_170.xml Machine-Readable version of the Parenago Catalogue of stars in the area of the Orion Nebula 2171 II/171 Parenago Catalog of Stars in Orion Nebula Machine-Readable version of the Parenago Catalogue of stars in the area of the Orion Nebula P P Parenago Trudy Gos. Astron. Inst. im. Shternberga, 25 ??? ??? 1954 1954TrSht..25....1P Machine-Readable version of the Parenago Catalogue of stars in the area of the Orion Nebula O Yu Malkov Bull. Inf. CDS 40 13 1992 1992BICDS..40...13M V/73 : Emission-Line Stars of the Orion Population (Herbig+ 1988) III/177 : H-alpha emission stars in the Orion region (Wiramihardja+ 1993) Kholopov P.N., Samus' N.N., Frolov M.S., Goranskij V.P., Gorynya N.A., Kireeva N.N., Kukarkina N.P., Kurochkin N.E, Medvedeva G.I., Perova N.B., Shugarov S.Yu. 1985a, General Catalogue of Variable Stars, Fourth Edition, vol.I, Nauka, Moscow. (Catalog <II/139>) Kholopov P.N., Samus' N.N., Frolov M.S., Goranskij V.P., Gorynya N.A., Kazarovets E.V., Kireeva N.N., Kukarkina N.P., Kurochkin N.E, Medvedeva G.I., Perova N.B., Rastorguev A.S., Shugarov S.Yu. 1985b, General Catalogue of Variable Stars, Fourth Edition, vol.II, Nauka, Moscow. (Catalog <II/139>) Kholopov P.N., Samus' N.N., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kazarovets E.V., Kireeva N.N., Kukarkina N.P., Medvedeva G.I., Pastukhova E.N., Perova N.B., Shugarov S.Yu. 1987, General Catalogue of Variable Stars, Fourth Edition, vol.III, Nauka, Moscow. (Catalog <II/139>) Kukarkin B.V., Parenago P.P., Efremov Yu.I., Kholopov P.N. 1951, Catalogue of Suspected Variable Stars, Moscow. Parenago P.P. 1954, "Trudy Gosudarstvennogo Astronomicheskogo Instituta im Shternberga", vol.25. Magnitudes, photographic Nebulae Stars, variable The present catalogue is a machine-readable version of the catalogue of stars in the area of the Orion nebula, published by P.P. Parenago (1954). The sky area between 5h 24m and 5h 36m in right ascension (1900.0) and between -4 and -7 degrees in declination (1900.0), containing the Orion nebula, has been investigated in that work. Ten of variable stars in original Parenago (1954) catalogue had CSV numbers (Kukarkin et al., 1951) but since that time all of them were confirmed as variables and included in GCVS (Kholopov et al., 1985a&b, 1987). We superseded CSV-numbers by GCVS-names in the machine-readable version for the following stars: ------------------------------------------------ Number in CSV-number GCVS-name the catalogue ------------------------------------------------ 1605 606 V372 ORI 1613 607 V373 ORI 1635 608 V374 ORI 1713 609 V375 ORI 1748 610 V387 ORI 1762 100569 V376 ORI 1974 617 V377 ORI 2183 625 V388 ORI 2393 630 V380 ORI 2478 634 V381 ORI ------------------------------------------------
The Parenago Catalogue Member asterisk if star is a member. the asterisk is set if a star is a member of the Orion nebula, blank otherwise. Probably, not every member of the nebula is marked by '*', but as Parenago (1954) noted "it was better to omit some of them (members), than to include nonmember stars" (p.250). Altogether 634 stars have asterisks. --- Parenago Sequential number. --- m_Parenago Blank for one star There are two different stars with number 2617 in the catalogue: 2617 and 2617A. --- RAh Right Ascension 1900 (hours) h RAm Right Ascension 1900 (minutes) min RAs Right Ascension 1900 (seconds) s DE- Declination 1900 (sign) --- DEd Declination 1900 (degrees) deg DEm Declination 1900 (minutes) arcmin mpg Photographic magnitudes. Blank when the star is variable; in that case the corresponding designation from GCVS (Kholopov et al., 1985a&b, 1987) appears in columns 36-45. mag n_mpg Flag on mpg the flag has the following meaning: 'E' - if photographic magnitude represents approximate estimation of visual or infrared magnitudes; 'N' - if the star is in the nebula and its influence can be perceptible; 'S' - if the influence of the nebula is strong; blank otherwise. --- l_mpv '<' should be read as "mpv fainter than" --- mpv photovisual magnitudes, if existing mag GCVS Name of variable star in GCVS <II/139> --- SpType Spectral type the spectral type (if existing) is a mean value both from literature and from Parenago's classification. The peculiarities 'e', 'ea' (read "e alpha") and 'eb' (read "e beta") mean hydrogen emission at the moment of observations. --- Malkov O.Yu ? 1992, Francois Ochsenbein [CDS] 04-Oct-1997 Feb 25 UNKNOWN UNKNOWN The catalogue was keypunched at the CDS and was checked at the Soviet Center of Astronomical Data. It was documented by O.Yu. Malkov in 1992. * 04-Oct-1997: documentation standardized at CDS (F. Ochsenbein) II_171.xml A Reference Catalogue of Galactic Novae (Version 1990.0) 2173 II/173 A Reference Catalogue of Galactic Novae A Reference Catalogue of Galactic Novae (Version 1990.0) H W Duerbeck CDS Bull. No. 34, p. 127 ??? ??? 1988 1988BICDS..34..127D Novae The catalogue contains all objects known or believed to be novae at one time or the other. Objects that were later found to be spurious have been omitted. Please note that completeness was only attempted for novae, not for dwarf novae, X-ray novae etc.
Catalog of Novae Name Designation by coordinates (IRAS scheme) --- Object Definitive designation (Variable Star Cat.) --- RAh 1950.0 (hours) h RAm 1950.0 (min) min RAs 1950.0 (s) s DE- 1950.0 (Sign) --- DEd 1950.0 (degrees) deg DEm 1950.0 (') arcmin DEs 1950.0 (") arcsec Glon Galactic Longitude (degrees) deg Glat Galactic Latitude (degrees) deg omax Observed magnitude at outburst mag u_omax Uncertainty flag --- oband Spectral region (p,j,v,r,i,B) of Observed magnitude at outburst --- tmax True maximum magnitude Based on extrapolation, if deviating from Observed magnitude at outburst mag u_tmax Uncertainty flag --- tband Spectral region of True maximum magnitude --- n_mmin '[' for Lower Limit --- mmin Minimum magnitude mag u_mmin Uncertainty flag --- mband Spectral region of Minimum magnitude --- LCtype Light curve type in system of Duerbeck (PASP 93, 165 (1981)) --- T3 Time of decline through three magnitudes, counted from maximum, in days d Type Type of object NA = Fast nova, t3-time smaller than 100 days, spectroscopically confirmed NB = Slow nova, t3-time larger or equal than 100 days, spectroscopically confirmed NC = Extremely slow nova, typical time scale: decades N = Nova; light curve too poorly known to establish speed class The following additions are used: : = nova, not confirmed by spectroscopic observations ? = existence of object based on one photographic or a few independent visual observations ?? = existence based on no more than two visual observations Other types of variability (objects once announced to be novae, but reclassified after more observations were obtained): NR = Recurrent nova NL = Novalike variable (inhomogeneous group) UG = U Geminorum variable (dwarf nova) UGSS = U Geminorum variable, SS Cyg subclass UGSU = U Geminorum variable, SU UMa subclass UGZ = U Geminorum variable, Z Cam subclass UGWZ = U Geminorum variable, WZ Sge subclass (not yet official subclass) ZAND = Symbiotic variable (Z And type) XND = X-ray nova (transient) system consisting of a compact component and a dwarf or subgiant star with spectral type G to M M = Mira star (long-period variable of large amplitude) UV = UV Ceti type star (flare star) FU = FU Ori type star (pre-main sequence) SDOR = S Dor type star (Hubble-Sandage variable) ---------------------------------------------------------------------------- --- Year Year of outburst (if known) yr Designations of Novae Name Designation by coordinates (IRAS scheme) --- Object Definitive designation (GCVS) --- Nova Nova Designation --- NSV NSV Designation --- AN Provisional designation (AN) --- Obs Obs. designation --- DM BD/CoD designation --- HD HD designation --- Other Other designation --- Disc Discoverer --- N. G. Roman ADC/SSDOO 1997 Apr 01 This ReadMe is based on an Intro file prepared by Francois Ochsenbein of CDS. II_173.xml Near Infrared Photometry of a Sample of IRAS Point Sources 2177 II/177 Near IR Photometry of a Sample of IRAS Point Sources Near Infrared Photometry of a Sample of IRAS Point Sources P Fouque T Le Bertre N Epchtein F Guglielmo F Kerschbaum Astron. Astrophys. Suppl. Ser. 93 151 1992 1992A&AS...93..151F J/A+AS/99/31 : Guglielmo et al., 1993, 106 new IR Carbon stars in the IRAS Point Source Catalog. J/A+AS/106/397 : Kerschbaum and Hron, 1994, JHKL'M-photometry for 200 stars J/A+AS/113/441 : Kerschbaum, 1995, JHKL'M-photometry for 44 semi-regular variables source: Fouque P., Le Bertre T., Epchtein N., Guglielmo F,, and Kerschbaum F. 1992, Astron. Astrophys. Suppl. Ser. 93, 151 LRS: IRAS Science Team 1986, Astron. Astrophys. Suppl. Ser., 65, 607 Volk K., Cohen M. 1989, Astron. J. 98, 931 Val: Epchtein N., Le Bertre T., Lepine J.R.D., Marques dos Santos P., Matsuura O.T., Picazzio E. 1987, Astron. Astrophys. Suppl. Ser., 71, 39 VH: van der Veen W., Habing H.J. 1988, A&A 194, 125 Mass loss Photometry, classification Stars, carbon The results are given for the 516 sources that we have observed from La Silla (452 in the southern hemisphere, plus 64 in the range 0 to 20deg). For each source, the IRAS name is given followed by the epoch of observation (with the convention given in Table 1), the J, H, K, L', M magnitudes that we have obtained, then three classifications based on IRAS Low Resolution Spectra (LRS), IRAS broad-band photometry (VH) and the combination of IRAS broad-band photometry with our near-infrared photometry (Val), and, finally, one association.
data from table 2 IRAS IRAS PSC (Catalogue <II/125>) number --- Note '*' when there is a note in table 1c of the published paper (see remarks.dat) --- Epoch coded according to Table 1 Table 1: Epoch label in main --------------------- ------------- 13-07-89 to 20-07-89 1 10-08-89 to 16-08-89 2 08-09-89 to 17-09-89 3 12-06-90 to 14-06-90 4 01-07-90 to 05-07-90 5 25-04-91 to 03-05-91 10 --- Jmag magnitude mag Hmag magnitude mag Kmag magnitude mag L'mag magnitude mag Mmag magnitude mag LRS IRAS/LRS Low resolution spectra classification --- VH IRAS/VH broad band photometry classification --- Val Classification based on IRAS/VH and authors photometry (=1987A&AS...71...39E) --- Assoc Name of associated optical source --- comments on observations IRAS IRAS PSC number --- LRS LRS classification --- VH VH classification --- Val Val classification --- Assoc Association PK = Catalog of Galactic Planetary Nebulae --- rem Comment on observation --- intro.tex latex description Michel Creze, Francois Ochsenbein CDS mod. J.A.Watko ADC 1996 Aug 21 UNKNOWN UNKNOWN * 28-Jul-1992: table was kindly mailed by Thibaut Le Bertre <lebertre@obspm.fr>, upon request by Michel Creze (CDS Director) * 15-Nov-1995: ReadMe file standardized (F. Ochsenbein, CDS) * 21-Aug-1996: Table 1, remarks.dat, references added (J.A. Watko, ADC) II_177.xml A Catalogue of Linear Polarization Measurements for 5070 stars 2178 II/178 Linear polarization measurements for 5070 stars A Catalogue of Linear Polarization Measurements for 5070 stars D J Axon R S Ellis Mon. Not. R. Astron. Soc. 177 499 1976 1976MNRAS.177..499A II/34 : Polarization Catalogue of 7503 stars by Mathewson, Ford, Klare, Neckel and Krautter (1975BICDS..14..115M) Polarization The authors have collected and collated measurements of linear polarization of starlight from Hiltner, Smith, Hall, Behr, Appenzeller, Mathewson and Ford, Klare et al., and Schroeder. These are presented in a catalog for stars with reliable distances that lists the Stokes parameters Q and U. The galactic latitude and longitude and distance are also given. See the documentation by Nancy G. Roman, either in plain ascii (file adc.doc), or in LaTeX (doc.tex)
The catalogue of linear polarization HD identification --- QStokes Stokes parameter Q (see adc.doc) mag UStokes Stokes parameter U (see adc.doc) mag GLON Galactic longitude deg GLAT Galactic latitude deg Dist Distance pc Remarks Other identifications and remarks --- adc.doc Documentation by Nancy G. Roman in plain ascii doc.tex Documentation by Nancy G. Roman in LaTeX CDS Catalogues Service CDS 1994 Oct 31 UNKNOWN UNKNOWN * 31-Oct-1994: the "Distance" column has been realigned. II_178.xml Southern Spectrophotometric Standards. I 2179 II/179 Southern Spectrophotometric Standards. I + II Southern Spectrophotometric Standards. I M Hamuy A R Walker N B Suntzeff P Gigoux S R Heathcote M M Phillips Publ. Astron. Soc. Pacific 104 533 1992 1992PASP..104..533H Southern Spectrophotometric Standards. I M Hamuy A R Walker N B Suntzeff P Gigoux S R Heathcote M M Phillips Publ. Astron. Soc. Pacific 106 566 1994 1994PASP..106..566H Spectrophotometry Stars, standard M. Hamuy, et al. have compiled their observations of secondary and tertiary spectrophotometric standard stars for the southern hemisphere in the wavelength range 3300-7550 Angstroms. The observations were made using the RC spectrographs and CCD cameras on the 1.5m and 4m telescopes at CTIO. The machine-readable files contain monochromatic magnitudes vs. wavelength for 29 stars in ASCII and 31 stars in FITS format.
The author's observations of secondary and tertiary southern spectrophotometric standard stars have been used to generate computer-readable files containing monochromatic magnitudes vs. wavelength for the range 3300-7550 Angstroms. The authors modified the monochromatic fluxes of the secondary standards according to the calibration of Vega published in 1985 by D. S. Hayes, and adjusted the zero point of their energy distributions by matching their V(synthetic) magnitudes to the observed magnitudes. They have used these adjusted secondary standards to calculate new fluxes for the tertiary standards of Stone and Baldwin (1983). The catalog consists of 29 files of blue magnitudes vs. wavelength and 30 files each which contain magnitude vs. wavelength for different standard stars in the red and for the entire wavelength range. There are an additional two stars, HR 1903 and HR 2421, for which the data is only in FITS format. Information on the contents of the FITS files is contained in the FITS headers of those files.
List of stars contained in this catalog FileName Name of file (in directory) with intensities --- Name Star name --- RAh Right Ascension 2000 (hours) number=1 values taken from the SIMBAD data-base h RAm Right Ascension 2000 (minutes) number=1 values taken from the SIMBAD data-base min RAs Right Ascension 2000 (seconds) number=1 values taken from the SIMBAD data-base s DE- Declination 2000 (sign) number=1 values taken from the SIMBAD data-base --- DEd Declination 2000 (degrees) number=1 values taken from the SIMBAD data-base deg DEm Declination 2000 (minutes) number=1 values taken from the SIMBAD data-base arcmin DEs Declination 2000 (seconds) number=1 values taken from the SIMBAD data-base arcsec Bmag B magnitude number=1 values taken from the SIMBAD data-base mag Vmag V magnitude number=1 values taken from the SIMBAD data-base mag SpType Spectral class number=1 values taken from the SIMBAD data-base --- File for CD -32 9927 File for EG 21 File for EG 274 File for Fiege 110 File for Fiege 56 File for HR 1544 File for HR 3454 File for HR 4468 File for HR 4963 File for HR 5501 File for HR 718 File for HR 7596 File for HR 7950 File for HR 8634 File for HR 9087 File for LTT 1020 File for LTT 1788 File for LTT 2415 File for LTT 3218 File for LTT 1377 File for LTT 3864 File for LTT 4364 File for LTT 4816 File for LTT 6248 File for LTT 7379 File for LTT 745 File for LTT 7987 File for LTT 9239 File for LTT 9491 Blue file for CD -32 9927 Blue file for EG 21 Blue file for EG 274 Blue file for Fiege 110 Blue file for Fiege 56 Blue file for Hiltner 600 Blue file for HR 1544 Blue file for HR 3454 Blue file for HR 4468 Blue file for HR 4963 Blue file for HR 5501 Blue file for HR 718 Blue file for HR 7596 Blue file for HR 7950 Blue file for HR 8634 Blue file for HR 9087 Blue file for LTT 1020 Blue file for LTT 1788 Blue file for LTT 2415 Blue file for LTT 3218 Blue file for LTT 1377 Blue file for LTT 3864 Blue file for LTT 4364 Blue file for LTT 4816 Blue file for LTT 6248 Blue file for LTT 7379 Blue file for LTT 7987 Blue file for LTT 9239 Blue file for LTT 9491 Red file for CD -32 9927 Red file for EG 21 Red file for EG 274 Red file for Fiege 110 Red file for Fiege 56 Red file for Hiltner 600 Red file for HR 1544 Red file for HR 3454 Red file for HR 4468 Red file for HR 4963 Red file for HR 5501 Red file for HR 718 Red file for HR 7596 Red file for HR 7950 Red file for HR 8634 Red file for HR 9087 Red file for LTT 1020 Red file for LTT 1788 Red file for LTT 2415 Red file for LTT 3218 Red file for LTT 1377 Red file for LTT 3864 Red file for LTT 4364 Red file for LTT 4816 Red file for LTT 6248 Red file for LTT 7379 Red file for LTT 745 Red file for LTT 7987 Red file for LTT 9239 Red file for LTT 9491 lambda Central wavelength 0.1nm mag Monochromatic magnitude (see source reference) mag del_lam Bandpass bandwidth 0.1nm hr1903.fit FITS file for HR 1903 hr2421.fit FITS file for HR 2421 Nancy G. Roman NASA/ADC/SSDOO 1995 May 31 The staff of the ADC gratefully acknowledges the support of Dr. Mario Hamuy in making the data files available for distribution. The fits files have been included only for the records for which no ASCII data are available. The first work on this catalog at the ADC was by James. E. Gass who also wrote the first version of this document. UNKNOWN UNKNOWN The list of stars (file stars.dat) was added at CDS in July 1998, using the SIMBAD data-base. UNKNOWN UNKNOWN The computer-readable version of Southern Spectrophotometric Standards. I corresponds to the contents of tables 13 and 14 in the source reference (Hamuy et al. 1992). The HR stars are secondary standards. The data provided are monochromatic magnitudes for the ten secondary standards at steps of 16 Angstroms, which corresponds to the resolution of the authors' 1.5m spectra. The magnitudes are averages of all the observations gathered for these stars. The published version of this data contains error estimates and bandpasses flagged for the presence of telluric features. This information is not part of the computer-readable version. The remaining files contain monochromatic magnitudes for the tertiary standard stars calculated through 50 A bandpasses. As with the secondary standard files, errors and telluric feature flags which appear in the source reference are not part of the computer-readable files. For this reason, researchers are cautioned to review the source reference carefully before using these data. The only changes made to the files as received were right justify the first column and align decimals in the second one. The FITS files, which were also received, have been omitted if the ASCII file is present. II_179.xml uvby-beta photometry of high-Velocity and metal-poor stars 2180 II/180 uvby-beta photometry of metal-poor stars uvby-beta photometry of high-Velocity and metal-poor stars W J Schuster P E Nissen Astron. Astrophys. 222 69 1989 1989A&A...222...69S J/A+AS/97/951 : a second catalogue by Schuster et al. =1993A&AS...97..951S Stars, high-velocity Stars, metal-deficient Galaxy: evolution Galaxy: halo stars: metallicity stars: ages Using the calibrations derived by Schuster and Nissen (=1989A&A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] <= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) > 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.
The Catalogue Name Star designation (HD/DM/Giclas) number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). --- RAh Right Ascension 1950 number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). h RAm Right Ascension 1950 number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). min RAs Right Ascension 1950 number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). s DE- Declination 1950 Sign number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). --- DEd Declination 1950 number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). deg DEm Declination 1950 number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). arcmin DEs Declination 1950 number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). arcsec E(b-y) Interstellar reddening number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). mag l_[Fe/H] '<' if [Fe/H] metallicity is an upper limit number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). --- [Fe/H] Metallicity (relative to Sun) number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). Sun Age Age in Giga-years number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). Ga e_Age rms error on Age number= G 266-060: common proper motion with G 226-061. HD 23439: double, component B is SB-CL, orbital elements by Latham et al. (=1988AJ.....96..567L). G 088-010: orbital elements by Latham et al. (=1988AJ.....96..567L). G 089-014: orbital elements by Latham et al. (=1988AJ.....96..567L). G 114-026: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 103095: double, orbital elements by Beardsley et al. (=1974ApJ...194..637B). G 065-022: orbital elements by Latham et al. (=1988AJ.....96..567L). HD 134439: common proper motion with HD 134440. G 141-019: orbital elements by Latham et al. (=1988AJ.....96..567L). G 206-034: orbital elements by Latham et al. (=1988AJ.....96..567L). G 026-009: double lined SB, orbital elements by Peterson et al. (=1980ApJ...239...50R). G 126-062: orbital elements by Latham et al. (=1988AJ.....96..567L). Ga Notes Remarks number=1 the following symbols are used in the remarks: AGB = asymptotic giant branch D = two stars in the diaphragm PHV = photometrically variable RHB = red horizontal branch RV-var = radial velocity variable SB-CL = spectroscopic binary (Carney + Latham, 1987, AJ 93, 116) SG = subgiant BS? = possible blue straggler * See Individual Notes --- Francois Ochsenbein CDS 1995 Nov 03 We thank Dr Poul E. Nissen for having supplied a copy of Table1. UNKNOWN UNKNOWN * 09-Sep-1992: table supplied by Poul E. Nissen <pen@obs.aau.dk> * 04-Jan-1993: First documentation at CDS (Francois Ochsenbein) * 03-Nov-1995: Documentation standardized at CDS, and notes added (Francois Ochsenbein) II_180.xml Atlas and Catalogue of IR Sources in the Magellanic Clouds 2181 II/181 Atlas and Cat IR Sources in the Magellanic Clouds Atlas and Catalogue of IR Sources in the Magellanic Clouds P B W Schwering F P Israel Kluwer Academic Publishers, Dordrecht/Boston/London ??? ??? 1990 1990acis.book.....S Infrared sources Magellanic Clouds Nebulae The authors have used the IRAS Sky Survey and Additional Observations data to construct an atlas of the Magellanic Clouds at wavelengths of 12, 25, 60, and 100 microns. These are contained in the published volume only. The position and characteristics of each infrared source identified in the maps are included in this compilation. Also included are cross references to sources at other wavelengths (H-alpha emission nebulae, dark clouds, and stars) when these could be reasonably identified with the IR sources. IRAS IDs (from the Point Source Catalog and the Small-Scale Structure Catalog) and the IRAS Additional Observation field numbers are also given.
Catalog of infrared point sources in the LMC and SMC Cld Cloud number=1 'L' for LMC or 'S' for SMC. --- Source Sequential source number number=2 Recommended prefixes: LI-SMC for the SMC sources and LI-LMC for the LMC sources. --- RAh Hours RA, equinox 1950.0 number=3 If a right ascension is given in 0.1s, it and the uncertainty are the same as in the IRAS PSC (IRAS. 1989); otherwise, right ascensions are taken from the DPM or Co-Add maps and the uncertainties are 12s. h RAm Minutes RA, equinox 1950.0 number=3 If a right ascension is given in 0.1s, it and the uncertainty are the same as in the IRAS PSC (IRAS. 1989); otherwise, right ascensions are taken from the DPM or Co-Add maps and the uncertainties are 12s. min RAs Seconds RA, equinox 1950.0 number=3 If a right ascension is given in 0.1s, it and the uncertainty are the same as in the IRAS PSC (IRAS. 1989); otherwise, right ascensions are taken from the DPM or Co-Add maps and the uncertainties are 12s. s DEd Declination (1950) number=4 If a declination is given in 1", it and the uncertainty are the same as in the IRAS PSC; otherwise, declinations are taken from the IRAS Additional Observation maps or the Co-Add maps and have uncertainties of 1'. deg DEm Declination (1950) number=4 If a declination is given in 1", it and the uncertainty are the same as in the IRAS PSC; otherwise, declinations are taken from the IRAS Additional Observation maps or the Co-Add maps and have uncertainties of 1'. arcmin DEs Declination (1950) number=4 If a declination is given in 1", it and the uncertainty are the same as in the IRAS PSC; otherwise, declinations are taken from the IRAS Additional Observation maps or the Co-Add maps and have uncertainties of 1'. arcsec I_12 12um intensity peak number=5 Blanks indicate that the source is below the intensity search level. The formats for the 25, 60, and 100um bands are variable: sometimes floating point, sometimes integer, and sometimes include '<' to indicate upper limits. 10-8W/m2/sr Bkgd_12 12um background 10-8W/m2/sr I_25 25um intensity peak number=5 Blanks indicate that the source is below the intensity search level. The formats for the 25, 60, and 100um bands are variable: sometimes floating point, sometimes integer, and sometimes include '<' to indicate upper limits. 10-8W/m2/sr Bkgd_25 25um background 10-8W/m2/sr I_60 60um intensity peak number=5 Blanks indicate that the source is below the intensity search level. The formats for the 25, 60, and 100um bands are variable: sometimes floating point, sometimes integer, and sometimes include '<' to indicate upper limits. 10-8W/m2/sr Bkgd_60 60um background 10-8W/m2/sr I_100 100um intensity peak number=5 Blanks indicate that the source is below the intensity search level. The formats for the 25, 60, and 100um bands are variable: sometimes floating point, sometimes integer, and sometimes include '<' to indicate upper limits. 10-8W/m2/sr Bkgd_100 100um background 10-8W/m2/sr Size Size number=6 The size of the source in right ascension (arcmin) x declination (arcmin). 'p' denotes a source that cannot be discerned from a point source response. A colon denotes an uncertain size. A dash indicates that no reliable size could be estimated because no FWHM could be determined. The size in these cases often agrees with a point source. The uncertainty in the source size is inversely proportional to the size itself, but no numberical value is derived. arcmin Fnu_12 Non-color corrected flux density, 12um number=7 Flux densities are derived on the assumption that the intrinsic source spectrum F(nu) is proportional to 1/nu. C denotes confusion with either background or other discrete sources and a colon indicates an uncertain flux density. Flux densities are calculated using the tabulated source Size. When the size could not be measured, the point source response was assumed. The error in flux densities is approximately 10-20% and depends on the intensity peak and background level. The flux densities have been obtained from maps produced with the November 1984 IRAS calibration (of the official IRAS products). Jy Fnu_25 Non-color corrected flux density, 25um number=7 Flux densities are derived on the assumption that the intrinsic source spectrum F(nu) is proportional to 1/nu. C denotes confusion with either background or other discrete sources and a colon indicates an uncertain flux density. Flux densities are calculated using the tabulated source Size. When the size could not be measured, the point source response was assumed. The error in flux densities is approximately 10-20% and depends on the intensity peak and background level. The flux densities have been obtained from maps produced with the November 1984 IRAS calibration (of the official IRAS products). Jy Fnu_60 Non-color corrected flux density, 60um number=7 Flux densities are derived on the assumption that the intrinsic source spectrum F(nu) is proportional to 1/nu. C denotes confusion with either background or other discrete sources and a colon indicates an uncertain flux density. Flux densities are calculated using the tabulated source Size. When the size could not be measured, the point source response was assumed. The error in flux densities is approximately 10-20% and depends on the intensity peak and background level. The flux densities have been obtained from maps produced with the November 1984 IRAS calibration (of the official IRAS products). Jy Fnu_100 Non-color corrected flux density, 100um number=7 Flux densities are derived on the assumption that the intrinsic source spectrum F(nu) is proportional to 1/nu. C denotes confusion with either background or other discrete sources and a colon indicates an uncertain flux density. Flux densities are calculated using the tabulated source Size. When the size could not be measured, the point source response was assumed. The error in flux densities is approximately 10-20% and depends on the intensity peak and background level. The flux densities have been obtained from maps produced with the November 1984 IRAS calibration (of the official IRAS products). Jy IRAS IRAS source name number=8 If the source is present in the IRAS Point Source Catalog (PSC; IRAS, 1989) or Small Scale Structure Catalog, its PSC/SSS designation is given. A colon indicates that the associated PSC or SSS entry is at a large distance from the source. An asterisk indicates that the association has been made for more than one source in the catalog. A plus sign indicates that another designation is given in the printed catalog. --- Field_no Field number in the accompanying Atlas of IRAS images of the SMC and LMC number=9 Field numbers are given for both the coadded IRAS sky survey images and the IRAS Additional Observations maps. --- Class Spectral code number=10 A single character indicating the spectral type of the source. Spectrum type 'C' is a 'cool dust' spectrum (typical Tdust about 30K), peaking beyond 100um; color correction factors are of order 1.00, 0.95, 0.99, and 1.00 (for 12, 25, 60, and 100um bands). Type 'W' is a 'warm dust' spectrum (typical Tdust about 70K), peaking between 12 and 100um; color correction factors are of order 1.03, 1.00, 1.00, and 1.04. Type 'S' is a 'stellar spectrum' (typical blackbody of about 5000K); color correction factors are of order 1.43, 1.40, 1.32, and 1.09. A semi-colon indicates that the infrared spectrum is uncertain. Actually, color-corrected flux densities can be calculated from the quoted ones by dividing the latter by these color correction factors. --- Information about positional associations with sources in other catalogs Assoc Record describing associations of sources in other catalogs, with format dependent on the catalog number=1 The six tables in the printed volume (two of which have three and five parts, respectively) that describe associations with sources in other catalogs have been concatenated into the single file assoc.dat here. The first byte in each record is an S or an L to indicate the cloud (SMC or LMC) in which the source is found. This is followed by one or more letters that indicate the type of source (see the first table below). Since the arrangement of the data is such that a character code is normally required to read it properly, no attempt was made to make the data arrangement in the various parts of the table correspond. However, the second table below lists the bytes in which each type of data is found for each type of source. Codes for Associations with Other Catalogs ------------------------------------------------------------- Code Meaning ------------------------------------------------------------- A Infrared emission from emission nebulae, Davies et al. (1976) D Infrared emission from Hodge (1972;1974) dark clouds S Infrared emission from stars in the SAO catalog K Infrared emission from star clusters, Kron (1956), Lindsay (1958) NGC Infrared emission from NGC clusters Sk Infrared emission from planetary nebulae, Sanduleak et al. (1978), Sanduleak and Pesch (1981) R Infrared emission from Radcliffe stars, Feast et al. (1960) N Infrared emission from supernovae remnants, Mathewson et al. (1983) ------------------------------------------------------------- Location of Data in Records of assoc.dat, by Source Type --------------------------------------------------------------- Source Code A D S K,R,N NGC Sk --------------------------------------------------------------- Type 1-2 1-2 1-2 1-2 1-4 1-3 Running No. 3-8 3-7 Source No. 9-20 3-8 6-7 6-9 6-7 LI No.* 26-38 11-18 14-18 15-18 15-18 Detection** 43 26 28 28 28 28 Intensity 21-24 Remarks 50-97 34-97 36-97 36-97 36-97 36-97 --------------------------------------------------------------- * This is the source number, SMC or LMC, in the present catalog. ** This is a single character indicating the certainty of the positional association. '+' means good; '0' means doubtful; '-' poor or absent. --- Nancy G. Roman, Gail L. Schneider, Seth W. Digel SSDOO/ADC 1997 Aug 22 UNKNOWN UNKNOWN Mar-1993: In addition to the concatenation described above, File 1 was modified in several ways. The file was reformatted to eliminate a number of blank columns. Plus signs were added to the IRAS identification to indicate an additional source in the printed catalog. Colons were added to the spectral types in the SMC where they appeared in the printed catalog. II_181.xml UBV Photometry of Stars whose Positions are Accurately Known 2182 II/182 UBV Photometry of Stars with Accurate Positions UBV Photometry of Stars whose Positions are Accurately Known T Oja Astron. Astrophys. Suppl. Ser. 57 357 1984 1984A&AS...57..357O UBV Photometry of Stars whose Positions are Accurately Known T Oja Astron. Astrophys. Suppl. Ser. 59 461 1985 1985A&AS...59..461O UBV Photometry of Stars whose Positions are Accurately Known T Oja Astron. Astrophys. Suppl. Ser. 61 331 1985 1985A&AS...61..331O UBV Photometry of Stars whose Positions are Accurately Known T Oja Astron. Astrophys. Suppl. Ser. 65 405 1986 1986A&AS...65..405O UBV Photometry of Stars whose Positions are Accurately Known T Oja Astron. Astrophys. Suppl. Ser. 68 211 1987 1987A&AS...68..211O UBV Photometry of Stars whose Positions are Accurately Known T Oja Astron. Astrophys. Suppl. Ser. 71 561 1987 1987A&AS...71..561O UBV Photometry of Stars whose Positions are Accurately Known T Oja Astron. Astrophys. Suppl. Ser. 89 415 1991 1991A&AS...89..415O UBV Photometry of Stars whose Positions are Accurately Known T Oja Astron. Astrophys. Suppl. Ser. 100 591 1993 1993A&AS..100..591O Photometry, UBV UBV photometry is presented for stars from AGK3R, NPZT, the Yale Bright Star Catalog (HR), and the FK5 faint extension. Stars with previously published UBV data were not selected. Observations were taken at the Kvistaberg Observatory and La Palma.
Mean errors are given in the latest paper as follows: for HR stars, 0.015 mag in V, 0.008 mag in B-V, 0.011 mag in U-B (U < 10), 0.027 mag in U-B (U > 10); for non-HR stars, 0.013 mag in V, 0.009 mag in B-V, 0.011 mag in U-B (U < 10), 0.031 mag in U-B (U > 10).
Catalog Data DMzone Durchmusterung zone (blank if HR) --- ID Star identification HR (four-digit number) CoD (zones -29deg to -23deg) BD (zone -22deg and northwards) --- IDsuf ID suffix --- V V magnitude mag B-V B-V color mag U-B U-B color if measured mag N Number of observations --- ref Source code (see References), S=standard star --- rem Remarks V = variable or suspected variable (for details see source paper) R = see source paper --- UNKNOWN 1993 standardized Julie Anne Watko [SSDOO/ADC] 30-May-1996 Mar 12 CDS thanks Dr T. Oja for having provided the files. II_182.xml UBVRI Photometric Standard Stars in the Magnitude Range 11.5 < V < 16.0 Around the Celestial Equator 2183 II/183 UBVRI Photometric Standards UBVRI Photometric Standard Stars in the Magnitude Range 11.5 < V < 16.0 Around the Celestial Equator A U Landolt Astron. J. 104 340 1992 1992AJ....104..340L Photometry, sequences Photometry, UBVRI UBVRI photoelectric observations have been made on the Johnson-Kron-Cousins photometric system of 526 stars centered on the celestial equator. The program stars within a 298 number subset have sufficient measures that they are capable of providing, for telescopes of intermediate and large size in both hemispheres, an internally consistent homogeneous broadband standard photometric system around the sky. The stars average 29 measures each on 19 nights. The majority of the stars in this paper fall in the magnitude range 11.5 < V < 16.0, and in the color range -0.3 < (B-V) < +2.3. Note: Tables 6 to 10 (filter sensitivities) were grouped into the "filters" file.
Standard Stars Star Star Designation TPHE = stars in the vicinity of T Phe ; (note that TPHE B = SW Phe) F = Feige PG = Palomar Green Two numbers indicate the "Durchmusterung of Selected Areas" (Harvard Annals 101) --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec V V mag B-V B-V mag U-B U-B mag V-R V-R mag R-I R-I mag V-I V-I mag n Number of observations --- m Number of nights --- e_V Mean error of the Mean V mag e_B-V Mean error of the Mean (B-V) mag e_U-B Mean error of the Mean (U-B) mag e_V-R Mean error of the Mean (V-R) mag e_R-I Mean error of the Mean (R-I) mag e_V-I Mean error of the Mean (V-I) mag Transmission Curves of CTIO's filter set No 3 (tables 6 to 10) Lambda Wavelength (Angstroems) 0.1nm T(U) Transmission in U filter % T(B) Transmission in B filter % T(V) Transmission in V filter % T(R) Transmission in R filter % T(I) Transmission in I filter % RCA 3103A photomultiplier No N49701 Lambda Wavelength 0.1nm AS Absolute sensitivity of RCA 3103A PM mA/W QE Quantum efficiency % Nancy G. Roman SDDOO/ADC 1995 Feb 15 This document was originally prepared by Francois Ochsenbein of the CDS. The undersigned has added a description and reformatted some of the material to make the document conform to the current standard. We appreciate Dr. Ochsenbein's transmitting both the files and the document to the ADC. II_183.xml 30 Doradus in the Large Magellanic Cloud: The Stellar Content and Initial Mass Function 2187 II/187 30 Doradus OB Associations 30 Doradus in the Large Magellanic Cloud: The Stellar Content and Initial Mass Function J W Parker Publ. Astron. Soc. Pac. 104 1107 1992 1992PASP..104.1107P Magellanic Clouds Clusters, open Photometry, UBV Johnson UBV photometry is presented for 2395 stars in the OB associations of 30 Doradus in the Large Magellanic Cloud. The CCD fields cover an area of 50 square arcminutes in the central region. The entire catalog (exclusive of the dense core cluster R 136) is photometrically complete to V = B = 18 mag and U = 17 mag, although the completeness magnitudes are fainter for regions with less nebular contamination.
These data have been reduced from 39 CCD frames (with short, medium, and long exposure times ranging from 3 to 1000 seconds) using the photometry program DAOPHOT written by Peter Stetson (1987, PASP, 99, 191). The photometric errors listed in these tables are the errors derived by DAOPHOT using the relative magnitude of the star on the CCD and the goodness of the fit of the point spread function. Most stars appear on more than one CCD frame per filter, and their resulting tabulated magnitudes are the averages of the individual measurements inversely weighted by the squares of their errors. The stars in these tables are from two regions: the central region and a non-overlapping northern region. The latter are designated by four digit numbers starting with 9. The X,Y coordinates are the positions relative to the northwestern-most corner of each region. The celestial coordinates have been calculated using full plate solutions of a few dozen stars measured on ESO sky survey plates and the X,Y coordinates from the catalogs.
Positional and photometric data Num Running number Stars without the suffix r are the Bluest (Q < -0.7) and Brightest (V < 16) Stars in 30 Doradus. --- RAh Right ascension 2000 h RAm Right ascension 2000 min RAs Right ascension 2000 s DE- Declination sign 2000 --- DEd Declination 2000 deg DEm Declination 2000 arcmin DEs Declination 2000 arcsec X X position coordinates are from the CCD finder charts in the reference Pixel sizes (in X and Y columns) are approximately 0.49 arcsec/pixel. pix Y Y position pix V V magnitude magnitudes and colors in the Johnson UBV system. mag B-V B-V color mag U-B U-B color 99.000 indicates no value for U-B mag e_V V accuracy mag e_B-V B-V accuracy mag e_U-B U-B accuracy 9.000 indicates no U-B value mag Spectroscopic data Num Running number Stars without the suffix r are the Bluest (Q < -0.7) and Brightest (V < 16) Stars in 30 Doradus. --- rej An r indicates a star too faint or red --- RAh Right ascension 2000 h RAm Right ascension 2000 min RAs Right ascension 2000 s DE- Declination sign 2000 --- DEd Declination 2000 deg DEm Declination 2000 arcmin DEs Declination 2000 arcsec X X position coordinates are from the CCD finder charts in the reference Pixel sizes (in X and Y columns) are approximately 0.49 arcsec/pixel. pix Y Y position pix V V magnitude magnitudes and colors in the Johnson UBV system. mag B-V B-V color mag U-B U-B color mag Q Q = (U-B) - 0.72(B-V) mag E(B-V) Color excess in B-V is the color excess calculated from Q as discussed in Section 2 of Paper II. mag Mv Absolute magnitude is the absolute V magnitude = V - Rv * E(B-V) - DM where Rv = 3.1, and the distance modulus DM = 18.5 mag. mag Teff Log effective temperature is the log10 of the effective temperature, and is calculated from Q or (B-V)0 as discussed in Section 3.1 of Paper II. K Mbol Bolometric magnitude is the bolometric magnitude = Mv + BC, where BC is calculated from Teff as discussed in Section 3.1 of Paper II. mag Sp Spectral type Sp. Type is the spectral type and luminosity class as determined from spectroscopic observations. One colon ":" indicates an uncertainty of one spectral subtype or luminosity class, and two colons "::" indicate a larger uncertainty. --- com Comments Comments are indicated by the following codes: a --- strong / over-subtracted Balmer lines b --- blend c --- possible composite / spectrum contaminated by nearby star e --- strong nebular emission in the Balmer lines f --- foreground star j,J --- has been observed by the author and the spectrogram appears in Figure 6 or 7 of Paper I. p --- peculiar (details in text of Paper I) m,M --- has been observed by Melnick (1985, A&A, 153, 235) w,W --- has been observed by Walborn (1986, IAU Symp. 116, 185; 1992 - unpublished classifications) or Walborn & Blades (1987, ApJ, 323, L65) z --- ZAMS O star The uppercase letters "J", "M", "W", indicate the sources of the spectral types listed in Column 14; two or all three letters may be uppercase if they agree on the same classification. --- Nancy G. Roman NASA/NSSDC/ADC 1994 May 17 UNKNOWN UNKNOWN * 17-May-1994: First archived * 15-Mar-1995: Corrected reference (PASP 104) and standardized this file (CDS) II_187.xml Long-Term Photometry of Variables at ESO. II. The Second Data Catalogue (1986-1990) 2188 II/188 Long-term photometry of Variables II Long-Term Photometry of Variables at ESO. II. The Second Data Catalogue (1986-1990) C Sterken J Manfroid K Anton A Barzewski E Bibo A Bruch M Burger H W Duerbeck R Duemmler A Heck H Hensberge M Hiesgen F Inklaar A Jorissen A Juettner U Kinkel Z Liu M V Mekkaden Y K Ng P Niarchos M Puttmann T Szeifert F Spiller R Van Dijk N Vogt I Wanders Astron. Astrophys. Suppl. Ser. 102 79 1993 1993A&AS..102...79S Long-Term Photometry of Variables at ESO. II. The Second Data Catalogue (1986-1990) C Sterken J Manfroid K Anton A Barzewski E Bibo A Bruch M Burger H W Duerbeck R Duemmler A Heck H Hensberge M Hiesgen F Inklaar A Jorissen A Juettner U Kinkel Z Liu M V Mekkaden Y K Ng P Niarchos M Puttmann T Szeifert F Spiller R Van Dijk N Vogt I Wanders ESO Sci. Report 12 ??? ??? 1993 1993ESOSR..12....1S II/170 : Long-Term Photometry of Variables at ESO I (1991) II/200 : Long-Term Photometry of Variables at ESO III (1995) II/202 : Long-Term Photometry of Variables at ESO IV (1995) Photometry, uvby Stars, variable The second catalogue of the LTPV programme contains photometric data obtained during the period October 1986 - September 1990. Full description can be found in ESO reports SP 8 and 12. The data presented here have been upgraded since the printing of catalogue ESO SR 12; a major change is the use of a quite different standard, namely the ESO SAT (Stroemgren Automatic Telescope) instrumental system has been used as standard. The instrumental systems 6 and 8 can be obtained by applying the following color matrices (see ESO SR 12, page 4, Eq. (3)), inverted (b-y , y , m1 , c1): SYSTEM 6 1.0518 0.0000 0.0000 0.0000 0.0094 1.0000 0.0000 0.0000 -0.1238 0.0000 1.1206 0.0000 0.0426 0.0000 0.0000 1.0352 SYSTEM 8 1.0476 0.0000 0.0000 0.0000 0.0384 1.0000 0.0000 0.0000 -0.0877 0.0000 1.0487 0.0000 -0.2657 0.0000 0.0000 0.9732 It also very easy to go back to the same standard as in ESO SR 8 by applying the transformations given in Table 3 of ESO SR 12 (page 3). Note that the faint star C7060 is not identified so far. The mean values of the r.m.s. deviations of the differential measurements of comparison stars are around (from Table 5 of paper) ------------------------------------ System y b-y m1 c1 ------------------------------------ 6 0.0069 0.0058 0.0122 0.0129 7 0.0064 0.0030 0.0039 0.0067 8 0.0068 0.0061 0.0110 0.0097 ------------------------------------
The observations Name Star Identification number=1 The cross-identifications are explained in "stars2" file. Program stars start with the letter P, and comparison stars with A, B ... --- HJD Heliocentric Julian Date d Airmass Airmass quantity (sec.z) --- u u magnitude mag v v magnitude mag b b magnitude mag y y magnitude mag T/S Telescope/system code --- R Release code --- Cross-identifications of observed stars Name Star Identification, as in file "ltpv2". --- HD HD designation --- HR HR (Bright Star) designation --- DM Durchmusterung (BD, CoD, CPD) designations --- Name2 Other designation --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Sp Spectral classification --- Francois Ochsenbein CDS 1995 Nov 27 UNKNOWN UNKNOWN * 07-Dec-1993: The catalogue was kindly provided to CDS by J.Manfroid * 27-Nov-1995: ReadMe file revisited at CDS (Francois Ochsenbein) "stars2" file expanded with J2000 positions. II_188.xml Supernova Studies: a Catalogue of magnitude observations of Type I Supernovae 2189 II/189 Magnitude Observations of Type I Supernovae Supernova Studies: a Catalogue of magnitude observations of Type I Supernovae R Cadonau B Leibundgut Astron. Astrophys. Suppl. Ser. 82 145 1990 1990A&AS...82..145C Supernovae Photometry, UBV Photometric observations (UBV or pg) of 81 supernovae of type I are presented. Only supernovae with multiple data are included. All SNe I for which observations in at least one of the four photometric filters, pg, B, V, and U could be found up to 1989 have been included. Most of the older SNe have been observed in the pg band whereas the B filter was used for more modern observations.
List of supernovae SN Supernova designation --- Galaxy Name of the galaxy --- GLAT Galatic latitude deg Abs Foreground absorptions in various bands toward the galaxy mag The catalogue of magnitude observations SN Name of the supernova, as in list.dat --- JD Julian date of the observations d m magnitude or color index mag u_m uncertainty flag [:] on m --- r_m reference of the magnitude (in file refs.dat) --- band magnitude band --- References of the magnitude observations ref Reference number --- text Text of reference --- paper.tex Table 2 of the publication in LaTeX Joseph Florsch CDS 1993 Dec 21 II_189.xml IRAS Minor Planet Survey (IMPS) 2190 II/190 IRAS Minor Planet Survey IRAS Minor Planet Survey (IMPS) E F Tedesco Phillips Laboratory, Technical Report No. PL-TR-92-2049. Hanscom Air Force Base, MA ??? ??? 1992 1992 II/126 : IRAS Serendipitous Survey Catalog (IPAC 1986) II/156A : IRAS Faint Source Catalog, |b| > 10, Version 2.0 II/174 : IRAS 2Jy Redshift Survey Data File VII/73 : IRAS Small Scale Structure Catalog VII/91 : IRAS Asteroid and Comet Survey (1986) VII/109 : IRAS Observations of Large Optical Galaxies VII/113 : Catalogued Galaxies + QSOs Observed in IRAS Survey IPAC 1986, Jet Propulsion Laboratory preprint JPL D-3698 The IRAS Minor Planet Survey (IMPS) Data Base, 1992 Infrared Astronomical Satellite, vol. 1 - Explanatory Supplement, NASA RP-1190 Minor planets Photometry, infrared The IRAS Minor Planet Survey (1992) supplements the asteroid data given in the IRAS Asteroid and Comet Survey (1986); comets are not included in IMPS. All asteroids with reasonably-well-known orbits as of December 1990 are covered. In particular, IMPS updates the processing of asteroids numbered 1 through 3318 and extends this processing to asteroid number 4679 plus 2,632 asteroids with preliminary (two or more opposition) orbits. IMPS processed only IRAS survey observations; Low Resolution Spectrometer, Serendipitous, and Additional Observations data were not processed. NOTE: The user is strongly advised to review the reference document and the Infrared Astronomical Satellite (IRAS) Explanatory Supplement.
*Albedos and Diameters *Singleton Data Base AstTyp Asteroid type --- AstID Asteroid identification number --- Name IAU designation --- Mv Absolute visual magnitude mag PHMean Mean visual albedo on the H, G system --- u_PHMean 1 sigma pH uncertainty --- DiaMean Mean diameter km u_DiaMean 1 sigma diameter uncertainty --- ProbLtCurv Probability lightcurve influenced sightings --- NUseSight Number of used sightings --- NUseObs Number of used observations (all bands) --- ratio Fraction-observed ratio --- stat1 Low position score See below. --- stat2 ADAS type 1 accept See below. --- stat3 ADAS type 1 reject See below. --- stat4 WSDB HCON position match See below. --- stat5 WSBM MCON position match See below. --- stat6 Small Scale Ver. 1 match See below. --- stat7 Relative flux out of bounds See below. --- stat8 IMPS asteroid association See below. --- stat9 Point source Ver. 2 match See below. --- stat10 Outer slot detection only See below. --- stat11 Predicted flux <0.14 Jy See below. --- stat12 Low detection rate FOR See below. --- stat13 12 mu albedo used See below. --- stat14 25 mu albedo used See below. --- stat15 60 mu albedo used See below. --- stat16 100 mu albedo used See below. --- stat17 Faint source Ver.2 match See below. --- stat18 25 mu flux < 1 Jy See below. --- stat19 Large albedo range See below. --- stat20 Serendipitous Ver. 1 match See below. --- stat21 -10 deg. < galactic latitude < +10 deg. See below. --- stat22 Galactic center match See below. --- stat23 ADAS type 2 now type 1 See below. --- stat24 Flux correction used See below. --- stat25 12 mu high density See below. --- stat26 25 mu high density See below. --- stat27 60 mu high density See below. --- stat28 100 mu high density See below. --- stat30 2+ known asteroid match See below. --- stat31 2+ sightings match See below. --- *Statistics AstTyp Asteroid type --- AstID Asteroid identification number --- Psight Predicted sightings --- Asight Accepted sightings --- Rsight Rejected sightings --- Msight Missed predicted sightings --- Fsight Too faint to expect a detection --- Dsight Dead 25 micron detector non-detections --- Nsight Noisy 25 micron detector non-detections --- Gsight Galactic center matches --- Osight Other non-detections --- *Reject AstTyp Asteroid type --- AstID Asteroid identification number --- Rsight Rejected sightings --- stat5 WCON sightings See below. --- stat9 PSC matches See below. --- stat10 Outer slots only See below. --- stat17 FSC matches See below. --- stat20 SSC matches See below. --- stat31 2+ sightings matches See below. --- Lsight Low position-match score --- B2sight Band-2-only with flux status < 5 --- Ssight Singletons with flux status < 5 --- CSsight Cross-scan uncertainty > 5 arcmin --- Cfail Color failures --- Qsight Confusion status failures --- CCfail Correlation coefficient failures --- Lalbedo Low albedos ( < 0.01 ) --- NCalbedo Albedo solutions not converged --- Ealbedo Albedo eliminated by Chauvenet criterion --- *Missed Predictions AstTyp Asteroid type --- AstID Asteroid identification number --- IAUName IAU designation --- NMiss No. of missed predicted scans --- Mv Absolute visual magnitude mag slope Slope parameter --- AlbEst Visual albedo estimate --- DiaMst Diameter estimate km AlbGLB Greatest lower albedo limit --- DiamLUB Least upper diameter limit km stat1 Low position score See below. --- stat2 ADAS type 1 accept See below. --- stat3 ADAS type 1 reject See below. --- stat4 WSDB HCON position match See below. --- stat5 WSBM MCON position match See below. --- stat6 Small Scale Ver. 1 match See below. --- stat7 Relative flux out of bounds See below. --- stat8 IMPS asteroid association See below. --- stat9 Point source Ver. 2 match See below. --- stat10 Outer slot detection only See below. --- stat11 Predicted flux <0.14 Jy See below. --- stat12 Low detection rate FOR See below. --- stat13 12 mu albedo used See below. --- stat14 25 mu albedo used See below. --- stat15 60 mu albedo used See below. --- stat16 100 mu albedo used See below. --- stat17 Faint source Ver.2 match See below. --- stat18 25 mu flux < 1 Jy See below. --- stat19 Large albedo range See below. --- stat20 Serendipitous Ver. 1 match See below. --- stat21 -10 deg. < galactic latitude < +10g. See below. --- stat22 Galactic center match See below. --- stat23 ADAS type 2 now type 1 See below. --- stat24 Flux correction used See below. --- stat25 12 mu high density See below. --- stat26 25 mu high density See below. --- stat27 60 mu high density See below. --- stat28 100 mu high density See below. --- stat30 2+ known asteroid match See below. --- stat31 2+ sightings match See below. --- *Ground-based Data AstTyp Asteroid type --- AstID Asteroid identification number --- IAUName IAU designation --- Mv Absolute visual magnitude mag slope Slope parameter --- AlbEst Estimated visual albedo (0.01 default) --- DiaMst Diameter estimate km TClass Taxonomic classification --- *Ground-based Data *Ground-based Data *Ground-based Data AstTyp Asteroid type --- AstID Asteroid identification number --- PJD Time (Julian Date) of perihelion passage d Mn Mean anomaly deg APn Argument of perihelion deg LAn Longitude of ascending node deg In Inclination deg En Eccentricity --- PDnAU Perihelion distance AU An Semimajor axis AU *Sightings AstTyp Asteroid type --- AstID Asteroid identification number --- ObsMonth Month of observation (year 1983) --- ObsDay Day of month of observation --- ObsHour Hour of observation (UTC) h ObsMin Minute of observation (UTC) min ObsSec Second of observation (UTC) s AstNam Sighting time tag 0.1s SOP SOP number --- OBS OBS number --- RAh Right ascension hours (observed) h RAm RA minutes min RAs RA seconds s DE- Sign of declination --- DEd Declination (observed) degrees deg DEm DEC minutes arcmin DEs DEC seconds arcsec AstGaC Celestial twist angle deg ELong Ecliptic longitude deg ELat Ecliptic latitude deg GLong Galactic longitude deg GLat Galactic latitude deg Hdist Heliocentric distance AU Gdist Geocentric distance AU PrdAlp Phase angle (negative before opp.) deg PRAh Right ascension hours (predicted) h PRAm RA minutes min PRAs RA seconds s PDEd Declination (predicted) degrees deg PDEm DEC minutes m PDEs DEC seconds s V Apparent visual magnitude mag Albed1 Derived visual albedo at 12 mu --- Albed2 Derived visual albedo at 25 mu --- Albed3 Derived visual albedo at 60 mu --- Albed4 Derived visual albedo at 100 mu --- u_Albed1 1-sigma uncertainties in Albedo at 12 mu --- u_Albed2 1-sigma uncertainties in Albedo at 25 mu --- u_Albed3 1-sigma uncertainties in Albedo at 60 mu --- u_Albed4 1-sigma uncertainties in Albedo at 100 mu --- Diam1 Diameter at 12 mu km Diam2 Diameter at 25 mu km Diam3 Diameter at 60 mu km Diam4 Diameter at 100 mu km u_Diam1 1-sigma uncertainties in Diam at 12 mu km u_Diam2 1-sigma uncertainties in Diam at 25 mu km u_Diam3 1-sigma uncertainties in Diam at 60 mu km u_Diam4 1-sigma uncertainties in Diam at 100 mu km *Sightings AstTyp Asteroid type --- AstID Asteroid identification number --- ObsMonth Month of observation (year 1983) --- ObsDay Day of month of observation --- ObsHour Hour of observation (UTC) h ObsMin Minute of observation (UTC) min ObsSec Second of observation (UTC) s AstSgY One sigma in scan uncertainty arcmin AstSgZ One sigma cross scan uncertainty arcmin AstLZ Cross scan uncertainty half width arcmin Score Position match score --- PosDiff Position difference |pred - obs| arcsec FCorr1 Low flux correction factor at 12 mu --- FCorr2 Low flux correction factor at 25 mu --- FCorr3 Low flux correction factor at 60 mu --- FCorr4 Low flux correction factor at 100 mu --- PrdFlx1 Predicted flux density at 12 mu Jy PrdFlx2 Predicted flux density at 25 mu Jy PrdFlx3 Predicted flux density at 60 mu Jy PrdFlx4 Predicted flux density at 100 mu Jy AstFlx1 Observed flux density at 12 mu Jy AstFlx2 Observed flux density at 25 mu Jy AstFlx3 Observed flux density at 60 mu Jy AstFlx4 Observed flux density at 100mu Jy AstSgF1 Flux density sigma at 12 mu Jy AstSgF2 Flux density sigma at 25 mu Jy AstSgF3 Flux density sigma at 60 mu Jy AstSgF4 Flux density sigma at 100 mu Jy AstSNR1 Signal to noise ratio at 12 mu --- AstSNR2 Signal to noise ratio at 25 mu --- AstSNR3 Signal to noise ratio at 60 mu --- AstSNR4 Signal to noise ratio at 100 mu --- *Sightings AstTyp Asteroid type --- AstID Asteroid identification number --- ObsMonth Month of observation (year 1983) --- ObsDay Day of month of observation --- ObsHour Hour of observation (UTC) h ObsMin Minute of observation (UTC) min ObsSec Second of observation (UTC) s AstDts1 Detector id array at 12 mu These are explained in detail in the IRAS Explanatory Supplement, pp X-12 - X-15. The corresponding notations are: AstDts = DETID AstCor = CORR AstCst = CSTAT AstFSt = FSTAT --- AstDts2 Detector id array at 25 mu These are explained in detail in the IRAS Explanatory Supplement, pp X-12 - X-15. The corresponding notations are: AstDts = DETID AstCor = CORR AstCst = CSTAT AstFSt = FSTAT --- AstDts3 Detector id array at 60 mu These are explained in detail in the IRAS Explanatory Supplement, pp X-12 - X-15. The corresponding notations are: AstDts = DETID AstCor = CORR AstCst = CSTAT AstFSt = FSTAT --- AstDts4 Detector id array at 100 mu These are explained in detail in the IRAS Explanatory Supplement, pp X-12 - X-15. The corresponding notations are: AstDts = DETID AstCor = CORR AstCst = CSTAT AstFSt = FSTAT --- AstCor1 Correlation coefficients at 12 mu --- AstCor2 Correlation coefficients at 25 mu --- AstCor3 Correlation coefficients at 60 mu --- AstCor4 Correlation coefficients at 100 mu --- ADStat1 Derived status word bits at 12 mu The detailed meaning of these quantities are unclear. --- ADStat2 Derived status word bits at 25 mu The detailed meaning of these quantities are unclear. --- ADStat3 Derived status word bits at 60 mu The detailed meaning of these quantities are unclear. --- ADStat4 Derived status word bits at 100 mu The detailed meaning of these quantities are unclear. --- AstCSt1 Confusion status word bits at 12 mu --- AstCSt2 Confusion status word bits at 25 mu --- AstCSt3 Confusion status word bits at 60 mu --- AstCSt4 Confusion status word bits at 100 mu --- AstFSt1 Flux status word at 12 mu --- AstFSt2 Flux status word at 25 mu --- AstFSt3 Flux status word at 60 mu --- AstFSt4 Flux status word at 100 mu --- stat1 Low position score See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat2 ADAS type 1 accept See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat3 ADAS type 1 reject See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat4 WSDB HCON position match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat5 WSBM MCON position match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat6 Small Scale Ver. 1 match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat7 Relative flux out of bounds See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat8 IMPS asteroid association See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat9 Point source Ver. 2 match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat10 Outer slot detection only See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat11 Predicted flux <0.14 Jy See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat12 Low detection rate FOR See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat13 12 mu albedo used See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat14 25 mu albedo used See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat15 60 mu albedo used See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat16 100 mu albedo used See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat17 Faint source Ver.2 match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat18 25 mu flux < 1 Jy See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat19 Large albedo range See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat20 Serendipitous Ver. 1 match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat21 -10 deg. < galactic latitude < +10 deg. See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat22 Galactic center match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat23 ADAS type 2 now type 1 See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat24 Flux correction used See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat25 12 mu high density See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat26 25 mu high density See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat27 60 mu high density See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat28 100 mu high density See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat30 2+ known asteroid match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- stat31 2+ sightings match See below. stat1 = Set if the parameter {[log(10)(SCORE)-3]/6} is less than 0.5. Sightings with a value less than 0.4 are also rejected. This parameter is a measure of the difference between the predicted and observed positions for an asteroid association. stat2 = Set for all sightings of an asteroid with identification number less than 3318 which was accepted in ADAS (Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat3 = Set for all sightings of an asteroid with identification number less than 3318 which was rejected in ADAS Infrared Astronomical Satellite Asteroid and Comet Survey, 1986). stat4 = Set for HCON (hours confirmed WSDB reject) asteroid sighting. stat5 = All MCON (WSDB "weeks" or months confirmed) asteroid sightings are rejected by IMPS (cf., stat9). stat6 = Set to indicate resolved spatial structure (cf., IRAS Small Scale Structure Catalog, 1986). stat7 = Set if the ratio of observed to predicted flux density at 25 mu is either less than 0.3 or greater than 3.0. stat8 = Set to unity for every asteroid sighting processed by IMPS. stat9 = All asteroid sightings confused with sources in the IRAS Point Source Catalog (IRAS Explanatory Supplement, 1985) are rejected by IMPS (subset of stat5. stat10 = All asteroid outer slot sightings are rejected by IMPS. stat11 = Set a priori for all candidate associations of an IMPS asteroid if no predicted flux density at 25 mu is greater than 0.14 Jansky. stat12 = Set for all sightings of each asteroid if the rate of successful detections (i.e., the fraction observed ratio FOR [(number used in FPard)/(number used + number missed)] is less than 0.3. stat13 = 12 mu albedo used stat14 = 25 mu albedo used stat15 = 60 mu albedo used stat16 = No 100 mu detections contribute to derived IMPS average values. stat17 = All asteroid sightings confused with sources in the IRAS Faint Source Survey (IRAS Faint Source Survey, 1989) are rejected by IMPS. stat18 = There are 1,267 accepted asteroids with no 25 mu observation of flux density greater than 1 Jansky used in their final IMPS derived average products. stat19 = Set for all sightings of an accepted asteroid if the ratio {[max- min]/[(max+min)/2]} ~ is greater than 0.75 for all derived albedos used in the final IMPS average. stat20 = All asteroid sightings confused with sources in the IRAS Serendipitous Survey Catalog (IRAS Serendipitous Survey Catalog, 1986) are rejected by IMPS . stat21 = Set if sighting within the galactic plane, i.e., not covered by the IRAS Faint Source Survey (cf., stat17). stat22 = Asteroid 25 mu only sightings are rejected by IMPS if near the galactic center +/3 deg. latitude by +/- 10 deg. longitude (subset of stat21). stat23 = Set if provisional asteroid elements updated and numbered since 1985. stat24 = Set if IMPS decreased (low) flux densities to compensate for IRAS bias near its SNR cutoff. stat25 = Set if sighting within an IRAS 12 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near the galactic center (cl., stat26). stat26 = Set if sighting within an IRAS 25 mu High Source Density Region (IRAS Explanatory Supplement, 1985) near galactic center (cl., stat25). stat27 = Set if sighting within an IRAS 60 mu High Source Density Region (IRAS Explanatory Supplement, 1985) of low galactic latitude near the center and anticenter. stat28 = Set if sighting within an IRAS 100 mu High Source Density Region (IRAS Explanatory Supplement, 1985) around the galactic center and anti-center. stat30 = Set if sighting associated with more than one asteroid prediction. stat31 = Set if more than one source is associated with a single asteroid prediction and therefore rejected by IMPS. --- N. G. Roman ADC/SSDOO 1997 Oct 31 This ReadMe is based partly on one prepared by J. Lyu and modified by M. Larkin. The undersigned thanks Dr. Tedesco for answering various questions about the data that were unclear in the reference. II_190.xml UBV Photometry of Barium Stars 2192 II/192 UBV Photometry of Barium Stars UBV Photometry of Barium Stars E Watanabe M Yutani Y Yamashita Publ. Nat. Astron. Obs. Japan 3 1 1993 1993PNAOJ...3....1W V/81 : Taxonomy of Barium Stars (Lu 1991) Photometry, UBV Stars, barium Stars, late-type Magnitudes in V and B-V and U-B colors observed by the 91-cm telescope at Okayama are presented for 109 stars including both classical and marginal barium stars. The two-color diagram shows a fair amount of spread. This can be interpreted by interstellar reddening and variable amounts of line blocking effect. Both classical and marginal barium stars form a fairly homogeneous group.
The catalogue of UBV for Ba stars. HD/DM HD or DM (CD <I/114> South of -23d, BD <I/119>, <I/122> otherwise) --- RAh R.A. at 1900 (hours) (1900) h RAm R.A. at 1900 (minutes) min DE- Dec. at 1900 (sign) --- DEd Dec. at 1900 (degrees) (1900) deg DEm Dec. at 1900 (minutes) arcmin Vmag observed V magnitude mag e_Vmag mean error of observed V magnitude mag B-V observed B-V color mag e_B-V mean error of observed B-V color mag U-B observed U-B color mag e_U-B mean error of observed U-B color mag Nobs number of nights observed --- Group certain or marginal Ba star See MacConnell D.J., Frye R.I. and Upgren A.R.: 1972 Astron. J., 77, 384 (1972AJ.....77..384M) --- SpType Spectral type See Yamashita Y. and Norimoto Y.: 1981, Ann. Tokyo Astron. Obs., 2nd Ser., 18, 125, 1981. (1981AnTok..18..124Y) --- S.Nishimura ADAC/NAOJ 1994, rev. F.Ochsenbein [CDS] 04-Oct-1997 Aug 29 II_192.xml A photometric study of the open cluster IC 4665 2194A II/194A Photometric study of IC 4665 A photometric study of the open cluster IC 4665 M F S J McCarthy S S J O'Sullivan Ricerche Astron. 7 483-498 1969 1969RA......7..483M Clusters, open Photographic catalog Photographic observations of the open cluster IC 4665 made on blue and yellow sensitive plates with the Vatican 40 cm refractor are presented and discussed. Apparent magnitudes were determined for 200 stars by means of a program of photometric reduction designed by BERTIAU. The mean internal errors in the final blue and yellow magnitudes average about 0.02 mag. All stars selected for measurement of proper motions by VASILEVSKIS on long base-line Allegheny plates have been observed here. The forty stars which VASILEVSKIS' proper motion measures have shown to be probable members constitute a normal main sequence from V = 7 to V = 13.5, followed by a gap of 0.2 to 0.3 mag, and a group of 10 stars in the subgiant domain. The reality of this gap and the membership characteristics of the stars in the subgiant region of the C - M diagram are discussed.
Standard stars: photoelectric and photographic data compared Vno Number on the plate (Vasilevskis) --- Kno Number in Kopff --- Ano Number in Alcaino --- BD Bonner Durchmustering identification --- Vpe V photoelectric mag (B-V)pe (B-V) color photoelectric mag Vpg V photographic mag (B-V)pg (B-V) photographic mag Notes Notes as follows: 1 = pe data from Hogg & Kron, AJ 60, 365 2 = pe data from Johnson ApJ 119, 181 and ApJ 126, 121 3 = pe data (this paper) 4 = pe data from Coyne (priv. comm.) 5 = not used as yellow standard --- General catalogue of stars observed in IC 4665 (Merging of tables 2,3,4) Vno Number on the plate (Vasilevskis) --- Kno Number in Kopff --- Ano Number in Alcaino --- BD Bonner Durchmustering identification --- B Photographic B mag V photographic V mag (B-V) color mag e_B mean error on B mag e_V mean error on V mag Class 1=probable member, 2=Possible member, 3=Less possible member --- Notes Notes as follows: #1 = Less than 6 plates in B determination #2 = Less than 6 plates in V determination #3 = Identification from Kopff, Mitt. Hamburger Sternw. 8, No 52 #4 = Suspected variable #6 = Photoelectric data from Hogg & Kron, AJ 60, 365 --- M.-J. Wagner, James Marcout, Francois Ochsenbein CDS 1995 Jun 12 UNKNOWN UNKNOWN * 02-Jun-1994: Keypunched at CDS, Strasbourg. Tables 2, 3 and 4 merged into single file table2. * 13-Jun-1995: errors corrected in table2 at CDS Star 093 Ano is 25 (instead of 26) Star 090 is BD+5 3483 (instead of BD+5 3843) Star 105 Ano is 24 (instead of 4) Star 033 Kno is 37 (instead of 38) II_194A.xml Interstellar extinction in the vicinity of the North America and Pelican nebulae 2196 II/196 Vicinity of North America and Pelican nebulae Interstellar extinction in the vicinity of the North America and Pelican nebulae V Straizys A Kazlauskas K Cernis V Vansevicius Baltic Astron. 2 171 1993 1993BaltA...2..171S Photometry, Vilnius Extinction Nebulae North America Nebula Pelican Nebula interstellar extinction dark clouds photometry: Vilnius stars: classification The results of photoelectric photometry of 564 stars in the Vilnius seven-color system in three areas near the North America and Pelican nebulae are given. Photometric spectral types, absolute magnitudes, colour excesses, interstellar extinctions and distances of the stars are determined. We find that the dark cloud separating both nebulae is at 580pc distance. A number of stars immersed into the dark cloud have been found. It seems that the dark cloud extends to south down to 40deg declination. The area southwest of {alpha} Cyg in the declination zones 42 and 43deg is comparatively transparent at least up to 1kpc.
Results of photometry in the dark cloud area Seq Sequential number --- n_Seq Individual note, see number=1 Individual notes: 2. Photometrically peculiar. 12. Classification uncertain. 14. Visual binary, measured together. 35. Visual binary. 53. Classification uncertain. 56. Classification impossible. 83. Mild subdwarf? 84. Classification uncertain. 89. Classification impossible. 95. Classification uncertain. 96. Classification impossible. 121. Visual binary, measured together. 122. Classification impossible, binary? 123. Photometric classification gives sdF5. The star cannot be of B-type since in that case it shows too large reddening for its distance. 126. Visual binary. 128. Classification uncertain. 137. Visual binary. 144. Visual binary. 146. 43 3769, visual binary, sep=1.0", measured together. 148. 42 3916, visual binary? 165. Classification uncertain. 184. Very red, classification uncertain, probably a carbon star. 186. 42 3924, visual binary ADS 14498 AB, sep=5.4", DELTAm~=4.0, measured together. 188. 42 3925, visual binary ADS 14497 AB, sep=8.6," DELTAm~=1.0, measured together. 206. Very red, classification impossible. --- BD BD designation --- Metik Metik number (Metik, 1960) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DEd Declination 1950 deg DEm Declination 1950 arcmin Split Spectral type from litterature number=2 Spectral types from literature are taken from HD, AGK3, Ikhsanov (1959), Jaschek (1978) and Metik (1960) --- Spphot Photometric spectral type (this paper) --- Vmag V magnitude (Vilnius system) mag u_Vmag uncertainty flag on Vmag --- U-P U-P colour index (Vilnius system) mag u_U-P uncertainty flag on U-P --- P-X P-X colour index (Vilnius system) mag u_P-X uncertainty flag on P-X --- X-Y X-Y colour index (Vilnius system) mag u_X-Y uncertainty flag on X-Y --- Y-Z Y-Z colour index (Vilnius system) mag u_Y-Z uncertainty flag on Y-Z --- Z-V Z-V colour index (Vilnius system) mag u_Z-V uncertainty flag on Z-V --- V-S V-S colour index (Vilnius system) mag u_V-S uncertainty flag on V-S --- n Number of independent observations --- Results of photometry in the area 40deg-41deg Results of photometry in the area 42deg-43deg Seq Sequential number --- n_Seq Individual note number=1 Individual notes: For table3: 1. 40 4103, visual binary, ADS 13672 AB, sep=2.7", DELTAm=2.5, O9+B2. 2. 40 4115, elliptical variable V470 Cyg, SB, B2+B2. If both components are of the same absolute magnitude their apparent magnitudes are 7.66 and the distance 432 pc. 7. 40 4124, Herbig Ae/Be star. 11. 40 4136, SB, G5 III+A. 37-38. 40 4197, visual binary, BDS 10274, sep=14.0", measured separately. 49. 40 4220, V729 Cyg, eclipsing binary, sep=1.5", DELTAm~=4.0. 52. 40 4227, visual binary ADS 14000 AB, sep=9.6", DELTAm~=1.0. 69. 40 4266, visual binary ADS 14126 AB, sep=0.6", Bp (Jaschek and Egret, 1982). 108. 40 4354, visual binary ADS 14413 AB, sep=5.8", DELTAm~=4.0. 111. 40 4358, visual binary ADS 14435 AB, sep=6.0", DELTAm~=3.5. 115. 40 4372, determination of M_V uncertain, A_V~=1.3mag. 125. 40 4393, suspected variable YZ Cyg. 127. 40 4399, visual binary ADS 14605 AB, sep=6.8", DELTAm~=3.5. 152. 41 3728, visual binary. 154. 41 3731, Herbig Ae/Be star. 158. 41 3737, visual binary ADS 13832 AB, sep=7.3", DELTAm~=5.0, measured together. 165. 41 3752, visual binary ADS 13869 AB, sep=1.4", DELTAm~=0.2. 184. 41 3796, visual binary ADS 13985 AB, sep=1.5", DELTAm~=0.8. 185. 41 3799, SB. 193. 41 3815, photometrically peculiar, A_V~=2.2mag. 201. 41 3844, visual binary ADS 14130 AB, sep=0.8", DELTAm~=2.0. 215. 41 3884A, visual binary ADS 14295 AC, sep=5.6", DELTAm~=3.5. 216. 41 3884B visual binary ADS 14295 B, about 10arcsec from component A. 217. 41 3889, visual binary ADS 14306 AB, sep=0.4", DELTAm~=1.0. 218. 41 3890, visual binary ADS 14308 AB, sep=4.5", DELTAm~=3.5. 232. 41 3932 visual binary ADS 14432 AB sep=2.9", DELTAm~=2.5. 244. 41 3962, also possible classification as sdF5. 245. 41 3962a, a star ~30arcsec from the BD 41 3962 star. 251. 41 3986, visual binary BDS 10719 BC, sep=7.3", DELTAm~=4.0 . 252. 41 3987, visual binary component BDS 10719 A. For table4: 8. 42 3684, photometric classification indicates a carbon star. 9. 42 3685, visual binary ADS 13689 AB, sep=0.9", DELTAm=~3.0. 21. 42 3718, visual binary ADS 13782 AB, sep=3.7", DELTAm=~3.0. 23. 42 3721, visual binary ADS 13786 AB, sep=1.0", DELTAm=~5.0. 25. 42 3724, visual triple component ADS 13786 C. 61. 43 3571, visual binary ADS 13736 AB, sep=5.8", DELTAm=~8.0, measured together. 62. 43 3573, visual triple ADS 13748 ABC, AB sep=0.2", DELTA}m=~0.2. 63. 43 3576, visual binary component ADS 13753 A. 72. 43 3598, visual binary ADS 13845 AB, sep=0.8", DELTAm=~2.0. 84-85. 43 3627, visual binary components ADS 13933 A and B, sep=~10", measured separately. 87. 43 3634, visual binary ADS 13959 AB, sep=2.8", DELTAm=~1.5. --- BD BD designation --- m_BD Multiplicity index on BD number --- HD HD designation --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DEd Declination 1950 deg DEm Declination 1950 arcmin Sp Spectral type from litterature number=2 Spectral types from literature are taken from HD, AGK3, compilations by Jaschek et al. (1964), Jaschek (1978), Goy (1973) and from the catalogues by Wilson (1953), Ikhsanov (1959, Malmquist et al. (1960). --- SpPhot Photometric spectral type --- Vmag V magnitude (Vilnius system) mag u_Vmag uncertainty flag on Vmag --- U-P U-P colour index (Vilnius system) mag u_U-P uncertainty flag on U-P --- P-X P-X colour index (Vilnius system) mag u_P-X uncertainty flag on P-X --- X-Y X-Y colour index (Vilnius system) mag u_X-Y uncertainty flag on X-Y --- Y-Z Y-Z colour index (Vilnius system) mag u_Y-Z uncertainty flag on Y-Z --- Z-V Z-V colour index (Vilnius system) mag u_Z-V uncertainty flag on Z-V --- V-S V-S colour index (Vilnius system) mag u_V-S uncertainty flag on V-S --- n Number of independent observations --- Quantification, extinction and distance determination in the dark cloud area Seq Sequential number --- Sp Spectral type --- Mv Absolute V magnitude mag u_Mv uncertainty flag on Mv --- Vmag V magnitude (Vilnius system) mag u_Vmag uncertainty flag on Vmag --- Av Visual extinction --- u_Av uncertainty flag on Av --- Dist Distance pc u_Dist uncertainty flag on Dist --- Quantification, extinction and distance determination in the 40deg-41deg area Quantification, extinction and distance determination in the 42deg-43deg area Seq Sequential number --- BD BD designation --- m_BD Multiplicity index on BD number --- Sp Spectral type --- Mv Absolute V magnitude mag u_Mv uncertainty flag on Mv --- Vmag V magnitude (Vilnius system) mag u-Vmag uncertainty flag on Vmag --- Av Visual extinction --- u_Av uncertainty flag on Av --- Dist Distance pc u_Dist uncertainty flag on Dist --- ant.tex TeX definitions ant2.tex TeX definitions ant3.tex TeX definitions ant4.tex TeX definitions bal.tex TeX definitions table2.tex TeX version of table2 table3.tex TeX version of table3 table4.tex TeX version of table4 table5.tex TeX version of table5 table6.tex TeX version of table6 table7.tex TeX version of table7 Patricia Bauer CDS 1994 Nov 24 Vytas Straizys <Valiauga.Astro@itpa.fi.lt> II_196.xml Radio continuum emission from stars: a catalogue update 2199A II/199A Radio continuum emission form stars Radio continuum emission from stars: a catalogue update H J Wendker Astron. Astrophys. Suppl. Ser. 109 177 1995 1995A&AS..109..177W Radio sources Stars, radio catalogs stars: general radio continuum: stars Radio data (1) Frequency in MHz (2) Maximun flux density in mJy (3) Minimun flux density in mJy. if =0, only one observation was made or the emission was steady (4) Code number of the reference (5) Remarks pertaining to the individual observations The following catalogue is an updated and changed version of the one first published in Abh.Hamburger Sternw. 1978, Vol.10, p 1ff. (CDS Catalogue II/129) A second version was contained in: Astron.Astrophys.Suppl. 1987, Vol.69, p 87 and microfiches (CDS Catalogue II/147). The basic concept of the earlier versions is preserved, namely one entry per star per frequency per paper. Space is now provided, however, to add more informations. These may be of technical or astronomical nature. Usually month and year of observation and the number of independent data points or length of monitoring session are given. All radio data are preceded by a header which contains information on the star or stellar system. (Note, that a physical stellar system is regarded as one single entry and that comments pertaining to individual components are found directly behind the observational data). Stellar data like names, position, proper motion, magnitudes and spectroscopic types are given in fixed format in a self-explanatory fashion. It is tried to have typical values from commonly available references. It is not intended to compete here with other compilations. These header informations are collected when the star is entered for the first time. They are only changed when new values are available while additional radio refences are added. An arbitrarily expandable section for unformatted text finishes the header. Finally, the units of the radio data remain in MHz (1.column) and mJy (2. and 3. columns). All coordinates refer to epoch and equinox 1950.0 (e.g. B1950). This is a so-called merged version e.g. all stars, those detected at least ones and those with upper limits only, are listed in order of ascending right ascension. The detected stars are marked with a "D" in the outermost right hand column in lines 1 to 5. The last updating occurred on 1994-Jul-01. In this version stars have new running numbers.
Positions and designations of the stars No Running number --- Name Main designation --- Alias Other name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Francois Ochsenbein, Patricia Bauer CDS 1998 Nov 26 UNKNOWN UNKNOWN * 08-Dec-1994: stored as received * 08-Feb-1995: the file "stars" is generated from "catalog" with positions and identifications of all 3021 stars * 26-Nov-1998: corrected file "stars.dat", several identifications found in error. II_199A.xml Long-Term Photometry of Variables at ESO. III. The Third Data Catalogue (1990-1992) 2200 II/200 Long-term photometry of Variables III Long-Term Photometry of Variables at ESO. III. The Third Data Catalogue (1990-1992) J Manfroid C Sterken B Cunow M De Groot A Jorissen R Kneer R Krenzin M Kruijswijk M Naumann M Niehues W Schoeneich M Sevenster N Vos N Vogt Astron. Astrophys. Suppl. Ser. 109 329 1995 1995A&AS..109..329M II/170 : Long-Term Photometry of Variables at ESO I (1991) II/188 : Long-Term Photometry of Variables at ESO II (1993) II/202 : Long-Term Photometry of Variables at ESO IV (1995) Photometry, uvby Stars, variable This is the third catalogue of photometric data in the Stroemgren system obtained during the period October 1990-January 1992 in the framework of the Long-Term Photometry of Variables (LTPV) program at the European Southern Observatory. All data have been obtained with the Danish 50-cm telescope. The mean values of the r.m.s. deviations of the differential measurements of comparison stars are around (from Table 4 of paper) ------------------------------ y b-y m1 c1 ------------------------------ 0.005 0.002 0.004 0.006 ------------------------------
The photometry Name Star Identification number=1 The cross-identifications are explained in "stars3" file. Program stars start with the letter P, and comparison stars with A, B ... --- HJD Heliocentric Julian Date d Airmass Airmass quantity --- umag u magnitude mag vmag v magnitude mag bmag b magnitude mag ymag y magnitude mag T/S Telescope/system code --- R Release code --- The stars observed Name Star Identification, as in "ltpv3" --- n_Name '*' indicates changes compared to the ESO publication (see "Historical Notes") --- HD HD designation --- HR HR (Bright Star) designation --- DM Durchmusterung (BD, CoD, CPD) designations --- Name2 Other designation --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Sp Spectral classification --- Francois Ochsenbein CDS 1995 Nov 27 UNKNOWN UNKNOWN * 01-Jun-1995: Corrections in file "stars3" in the electronic version: => P7073 and P7074 (CPD instead of BD) => P2003 (in Vol constellation instead of Vel). => B7070, A7071, B7071 were added. => A7070, P7070, A2027, P2027, P2027, B2027, A2028, P2028, B2028, B2028 Durchmusterung designations added => Designations of stars provided by Chris sterken <csterken@vub.ac.be> A7074 A7076 B7073 B7074 B7076 C5006 * 27-Nov-1995: HDJ dates converted to absolute values, and "ReadMe" file standardized at CDS II_200.xml Long-Term Photometry of Variables at ESO. IV. The Fourth Data Catalogue (1992-1994) 2202 II/202 Long-term photometry of Variables IV Long-Term Photometry of Variables at ESO. IV. The Fourth Data Catalogue (1992-1994) C Sterken J Manfroid D Beele S de Koff I M M G Eggenkamp K Goecking A Jorissen A Kaufer C Kuss A P Schoenmakers J M Still J van Loon J Vink S Vrielmann E Waelde Astron. Astrophys. Suppl. Ser. 113 31 1995 1995A&AS..113...31S II/170 : Long-Term Photometry of Variables at ESO I (1991) II/188 : Long-Term Photometry of Variables at ESO II (1993) II/200 : Long-Term Photometry of Variables at ESO III (1995) Photometry, uvby Stars, variable This is the fourth catalogue of photometric data in the Stroemgren system obtained during the period June 18, 1992 - August 23, 1994 in the framework of the Long-Term Photometry of Variables (LTPV) program at the European Southern Observatory. Since our goal is not absolute (all-sky) photometry, the observations should be used for differential photometry only. The mean values of the r.m.s. deviations of the differential measurements of comparison stars are around (from Table 3 of paper) ------------------------------ y b-y m1 c1 ------------------------------ 0.005 0.002 0.004 0.007 ------------------------------ Important Notice: The file "ltpv4" which was accessible at CDS before 20 October 1996 was incorrect.
*The observations Name Star Identification number=1 The cross-identifications are explained in "stars4" file. Program stars start with the letter P, and comparison stars with A, B ... --- HJD Heliocentric Julian Date d Airmass Airmass quantity (sec.z) --- ymag Stroemgren's y magnitude mag b-y Stroemgren's b-y colour mag m1 Stroemgren's m1 ((v-b)-(b-y)) colour mag c1 Stroemgren's c1 ((u-v)-(v-b)) colour mag T/S Telescope/system code ("N" is the "natural" system") --- The list of stars observed Name Star Identification, as in file "ltpv4". --- HD HD designation --- HR HR (Bright Star) designation --- DM Durchmusterung (BD, CoD, CPD) designations --- Name2 Other designation --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Sp Spectral classification --- Francois Ochsenbein CDS 1996 Oct 21 We thank Chris Sterken <csterken@vub.ac.be> for providing the original catalogue in LaTeX format. UNKNOWN UNKNOWN * The original LaTeX files were provided by Chris Sterken in LaTeX format in November 1995; an unfortunate error in the translation from latex to ascii made at CDS generated an erroneous "ltpv4" file, which was only detected in October 1996 thanks to Ali Moujtahid <moujtahi@mesioq.obspm.fr> * 21-Oct-1996: file "ltpv4" recreated at CDS. II_202.xml Second EUVE Source Catalog 2203 II/203 Second Extreme Ultra-Violet Explorer Catalog Second EUVE Source Catalog S Bowyer M Lampton J Lewis X Wu P Jelinsky R F Malina Astrophys. J. Suppl. Ser. 102 129 1996 1996ApJS..102..129B J/ApJS/93/569 : First EUVE source catalogue (Bowyer+, 1994) J/AJ/107/751 : EUV Explorer bright sources list (Malina+, 1994) http://www.cea.berkeley.edu/HomePage.html (Center for EUV Astrophysics) EUV sources The Extreme Ultraviolet Explorer satellite was launched on June 7, 1992 from Cape Canaveral, Florida on a Delta II rocket. The payload contains three EUV scanning telescopes equipped with imaging detectors as well as a Deep Survey Spectrometer instrument which divides the light from a fourth telescope between an imaging detector and three EUV spectrometers. There are three source tables in this catalogue: - table1 lists count rates and positions of 514 objects detected during the all-sky survey. - table2 lists 35 sources detected by the deep survey of half the ecliptic plane; three deep survey objects are also detected in the all sky survey. - table3 lists 188 sources that have been detected in other ways, principally by deep exposures with the scanner telescopes as part of the Right Angle Program or by long exposures with the deep survey instrument; table3 includes right angle detections through December 24, 1994. Because the objects listed in table3 have been derived with a variety of instruments and exposure strategies, the flux limits and detection thresholds vary over a wide range; interested readers should consult the reference listed. Each table has an associated list of identified sources, id1, id2 and id3 (one EUVE source may by associated to 0, one or more counterparts); in nearly all cases they lie within 1 arcmin of the actual source position.
EUVE
All-sky survey EUVE Catalog designation based on J2000 position --- RAh Best fit Right Ascension J2000 (hours) for detected EUVE source h RAm Best fit Right Ascension J2000 (minutes) min RAs Best fit Right Ascension J2000 (seconds) s DE- Best fit Declination J2000 (sign) for detected EUVE source --- DEd Best fit Declination J2000 (degrees) deg DEm Best fit Declination J2000 (minutes) arcmin c100A 100A (10nm) Lexan/boron band observed mean countrate ct/ks u_c100A indicates detections < 3 sigma --- e_c100A one sigma countrate error ct/ks c200A 200A (20nm) aluminium/carbon band observed mean countrate ct/ks u_c200A indicates detections < 3 sigma --- e_c200A one sigma countrate error ct/ks c400A 400A (40nm) multicomponent-filter band observed mean countrate ct/ks u_c400A indicates detections < 3 sigma --- e_c400A one sigma countrate error ct/ks c600A 600A (60nm) tin (Sn) band observed mean countrate ct/ks u_c600A indicates detections < 3 sigma --- e_c600A one sigma countrate error ct/ks Deep Survey of half the ecliptic plane EUVE Catalog designation based on J2000 position --- RAh Best fit Right Ascension J2000 (hours) for detected EUVE source h RAm Best fit Right Ascension J2000 (minutes) min RAs Best fit Right Ascension J2000 (seconds) s DE- Best fit Declination J2000 (sign) for detected EUVE source --- DEd Best fit Declination J2000 (degrees) deg DEm Best fit Declination J2000 (minutes) arcmin c100A 100A (10nm) Lexan/boron band observed mean countrate ct/ks u_c100A ')' indicates detections < 3 sigma --- e_c100A one sigma countrate error ct/ks c200A 200A (20nm) aluminium/carbon band observed mean countrate ct/ks u_c200A ')' indicates detections < 3 sigma --- e_c200A one sigma countrate error ct/ks Sources detected in other ways EUVE Catalog designation based on J2000 position --- RAh Best fit Right Ascension J2000 (hours) for detected EUVE source h RAm Best fit Right Ascension J2000 (minutes) min RAs Best fit Right Ascension J2000 (seconds) s DE- Best fit Declination J2000 (sign) for detected EUVE source --- DEd Best fit Declination J2000 (degrees) deg DEm Best fit Declination J2000 (minutes) arcmin c100A 100A (10nm) Lexan/boron band observed mean countrate ct/ks n_c100A indicates possible UV leak --- c200A 200A (20nm) aluminium/carbon band observed mean countrate ct/ks u_c200A indicates possible UV leak --- c400A 400A (40nm) multicomponent-filter band observed mean countrate ct/ks n_c400A indicates possible UV leak --- c600A 600A (60nm) tin (Sn) band observed mean countrate ct/ks n_c600A indicates possible UV leak --- c100DS DS100A (10nm) Lexan/boron band observed mean countrate ct/ks n_c100DS indicates possible UV leak --- c200DS DS200A (20nm) aluminium/carbon band observed mean countrate ct/ks n_c200DS indicates possible UV leak --- Identifications of table1 Identifications of table2 Identifications of table3 EUVE Catalog designation based on J2000 position --- Q Identification characterisation number=1 the `Q' column indicates our level of confidence in each source detection: Q=1 denotes likely identification on basis of known EUV emitter from previous work or from membership in a class of known EUV emitters. Q=2 denotes acceptable positional coincidence but little or no other supporting evidence. Q=U denotes some of the detected source counts originate from the known UV leak of one or more of the EUVE filters Q=H means no counterpart has been found, but the detection is statistically secure found, the detection is statistically secure in the sense of its satisfying the more stringent selection criteria. Q= (a blank) indicates that the detection lies in the less stringent group, and no other supporting evidence is available. --- Name1 ID name 1 --- Name2 ID name 2 --- Type ID spectral type or description --- MAG magnitude of ID object mag Sep angle separating EUVE & ID in arcsec arcsec Comments See note number=2 the following catalogue abbreviations are used: 1E =1979ApJ...234L...1G First Einstein survey (Giacconi et al.) 4U =1978ApJS...38..357F Fourth Uhuru catalog (Forman et al.) AF =1995ApJ...441..726F High Galactic Latitude Planetary Nebulae (Fruscione et al.), AF2 = X-Ray Selected EUV Galaxies (Fruscione A. 1995, ApJ, submitted) DK = D. Kilkenny M. Mathioudakis (1995 private communication) HM =1995ApJ...455..574D All-sky Survey (Marshall et al.) JD =1995ApJ...455..574D Hot White Dwarfs in the LISM (Dupuis et al.) JE =1995ApJ...454..442E Millisecond Pulsar J0437-4715 (Edelstein et al.) JF =1994BAAS...26..870F Middle Aged Pulsar PSR 0656+14 (Finley et al.) JL = Transient/Flaring EUV Sources (Lewis et al. 1995, Proc. EUV Colloq. 152, Berkeley CA) KM =1994AJ....108.1843M First Year of EUVE RAP (McDonald et al. 1994) LTT = Luyten 1957, "Catalogue of 9867 stars in the Southern Hemisphere with Proper Motion Exceeding 0.2" (Univ. Minnesota) Luyten 1961, "Catalogue of 7127 Stars in the Northern Hemisphere with Proper Motion Exceeding 0.2" (Univ. Minnesota) MM =1995A&A...300..775M Activity Versus Rotation (Mathioudakis et al.) NC = Optical ID of EUV Sources (Craig et al. 1995, ApJ, submitted) NC2 = N. Craig (1995 private communication) RE =1993MNRAS.260...77P Rosat WFC Catalog (Pounds et al.) RF = EUV Emission from Neutron Stars (Foster et al. 1995, Proc. EUV Colloq 152, UC Berkeley) RG =1995AJ....110..788G Field of EUVE J1027+323 (Genova et al. 1995) RL = EUV Emission of Active Galactic Nuclei (Lieu et al. 1995, Adv. Space Res., 16(3), 81) SV =1995ApJ...448L...9V EUV from Seyfert Ton S180 (Vennes et al.) TD1 =1983MNRAS.202..317C TD1 UV survey (Carnochan Wilson 1983; catalog <II/59>) --- Francois Ochsenbein CDS 1996 Feb 15 Dr. Nahide Craig <ncraig@cea.berkeley.edu> II_203.xml The Preliminary Version of the Bibliographic Catalogue of Stellar Polarization (BCSP) 2206 II/206 Stellar Polarization Bibliography The Preliminary Version of the Bibliographic Catalogue of Stellar Polarization (BCSP) M L Belous Bull. Inf. CDS 48 5 1996 1996BICDS..48....5B Polarization This preliminary version of Bibliographic Catalogue of Stellar Polarization (BCSP) contains data about polarization measurements of more than 1600 galactic objects published during the period 1977-1981. All the information included in the Catalogue has been taken from original papers published during this period. The main goal of the Catalogue is to present necessary bibliography to explorers studying a certain object and to give them some primary polarization data concerning with it. See the full documentation in file bcsp.doc (or bcsp.tex)
The Bibliographical Catalogue of Stellar Polarization *Stars without position Name Object identifier, preferably HD number=1 Object identifiers are mostly taken from the articles in which these objects are described; when absent, the coordinates are taken from SIMBAD. See also file bcsp.doc, section IV. The Greek letters designations used in the Catalogue are: +----------------------------------------------------------+ : Alpha ALP : Eta ETA : Nu NHU : Tau TAU : : Beta BET : Theta THE : Xi KSI : Upsilon UPS : : Gamma GAM : Iota IOT : Omicron OMI : Phi PHI : : Delta DEL : Kappa KAP : Pi PIE : Chi CHI : : Epsilon EPS : Lambda LAM : Rho RHO : Psi PSI : : Zeta ZET : Mu MHU : Sigma SIG : Omega OME : +----------------------------------------------------------+ --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin SpType Spectral type number=2 if an object spectrum was not presented in the original paper, it was taken from SIMBAD; see also file bcsp.doc, section IV. --- p The degree of polarization number=3 the degree of linear polarization as determined by authors, or converted from Stokes parameters. See byte 83 for circular polarization. See also file bcsp.doc, section V. % n_Filter '#' for unfiltered measurement --- Filter Names of Johnson-Morgan used filters number=4 the non-standard units are um micrometers (10-6m) A angstroms (10-10m) GH gigahertzs (10+9Hz) MH megahertzs (10+6Hz) kV kiloelectronvolts (keV) See also file bcsp.doc, section VI. --- oFilters Number of other used filters, or '>' if more than 20. ---- x_Lambda Units in which wavelengths are given number=4 the non-standard units are um micrometers (10-6m) A angstroms (10-10m) GH gigahertzs (10+9Hz) MH megahertzs (10+6Hz) kV kiloelectronvolts (keV) See also file bcsp.doc, section VI. --- Lambda1 Lower filter bordering (units are x_Lambda) --- Lambda2 Upper filter bordering (units are x_Lambda) --- circPol Circular polarization note number=5 the various polarization flags are described in file bcsp.doc, section VII. The 0 value means "absent" or "not explored". --- varPol Variability of polarization number=5 the various polarization flags are described in file bcsp.doc, section VII. The 0 value means "absent" or "not explored". --- lamPol Wavelength dependence polarization number=5 the various polarization flags are described in file bcsp.doc, section VII. The 0 value means "absent" or "not explored". --- spatPol Spatial polarization note number=5 the various polarization flags are described in file bcsp.doc, section VII. The 0 value means "absent" or "not explored". --- authPol Author's conclusion about polarization nature number=5 the various polarization flags are described in file bcsp.doc, section VII. The 0 value means "absent" or "not explored". --- m_ObsDate '*' when several observation periods number=6 n_obs takes the values 0 = duration not specified 1 = duration not more than 24 hours 2 = duration between 1day and 1month 3 = duration between 1month and 1year 4 = duration more than 1year See also file bcsp.doc, section VIII. --- n_ObsDate Indication about duration number=6 n_obs takes the values 0 = duration not specified 1 = duration not more than 24 hours 2 = duration between 1day and 1month 3 = duration between 1month and 1year 4 = duration more than 1year See also file bcsp.doc, section VIII. --- ObsDate Observation date number=6 n_obs takes the values 0 = duration not specified 1 = duration not more than 24 hours 2 = duration between 1day and 1month 3 = duration between 1month and 1year 4 = duration more than 1year See also file bcsp.doc, section VIII. --- Ref Reference (A&AA number), number=7 the references are collected in files gcpbc.bib (sorted by reference numbers) and authors.bib (sorted by authors). See also file bcsp.doc, section IX. --- Type Object type number=8 the object classes are explained in file bcsp.doc, section X. --- Name2 Another object identifier number=1 Object identifiers are mostly taken from the articles in which these objects are described; when absent, the coordinates are taken from SIMBAD. See also file bcsp.doc, section IV. The Greek letters designations used in the Catalogue are: +----------------------------------------------------------+ : Alpha ALP : Eta ETA : Nu NHU : Tau TAU : : Beta BET : Theta THE : Xi KSI : Upsilon UPS : : Gamma GAM : Iota IOT : Omicron OMI : Phi PHI : : Delta DEL : Kappa KAP : Pi PIE : Chi CHI : : Epsilon EPS : Lambda LAM : Rho RHO : Psi PSI : : Zeta ZET : Mu MHU : Sigma SIG : Omega OME : +----------------------------------------------------------+ --- References Ref Reference (A&AA number) --- Text Full text of reference --- bcsp.doc Documentation in ascii format bcsp.tex Documentation in LaTeX format Francois Ochsenbein CDS 1996 Apr 02 UNKNOWN UNKNOWN * 10-Jul-1995: paper submitted to CDS Information Bulletin * 02-Apr-1996: a few positions in file "nocoord.dat" were added at CDS, taken from SIMBAD or Durchmusterung catalogues. II_206.xml The Palomar-Green catalog of ultraviolet-excess stellar objects. 2207 II/207 Palomar-Green catalog UV-excess stellar objects The Palomar-Green catalog of ultraviolet-excess stellar objects. R F Green M Schmidt J Liebert Astrophys. J. Suppl. Ser. 61 305 1986 1986ApJS...61..305G J/AJ/111/645 : Morphology of Bright Quasars of this list (Fabian+ 1996) Ultraviolet Photometry, UBV Photometry, uvby Blue objects techniques: photometric quasars: general stars: faint blue stars: spectral classification stars: stellar statistics subdwarfs white dwarfs The Palomar-Green Catalogue of UV-excess stellar objects provides positions accurate to about 8arcsec in each coordinate, photographic B-magnitudes accurate to 0.29mag, spectral types, some cross-references, and photoelectric broad-band, multichannel, and Stroemgren colors when available. Of the 1874 objects in the catalogue as published in 1986 (1878 in this version), 1715 comprise a statistically complete sample covering 10714 square degrees from 266 fields taken on the Palomar 18-inch Schmidt telescope. Limiting magnitudes vary from field to field, ranging from 15.49 to 16.67. The overall completeness is estimated to be 84%, but that figure and the relative contributions of magnitude, color, and accidental errors vary depending on the magnitude and color distribution of the spectroscopic subsample.
*Palomar-Green Survey Data (Table 5) PG PG name number=1 This name did not exist in the original table; it has been built from RAh, RAm, DE-, DEd and a digit representing the rounded part of DEm. In the publication, these names appear only in the finding charts. *** Remark on PG 1535+547: its cross-identification in Zwicky catalog corrected (see History below) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Pmag Photographic magnitude, accuracy 0.29mag mag Blim Limiting magnitude of field number=2 if the object was found in overlapping fields, Blim indicates the deeper exposure. A value of 0. means that the object is not part of the complete statistical sample, which can be due to faintness, undetection in automated scanning process, or presence in a field with abnormally bright Blim. mag Comment Other names, redshift or spectral type number=3 this column contains redshifts for extragalactic sources, spectral types for companions to the blue stars, and brief notes about spectral peculiarities or uncertainties. It contains also cross-identifications of the objects. For white dwarfs, see the McCook & Sion catalog <III/129> For PHL (Palomar-Haro-Luyten, 1962BITon...3...37H) see catalog <III/74> EG = Eggen and Greenstein (1965ApJ...141...83E, 1967ApJ...150..927E) T = Tonantzintla lists (1957BOTT....2G...3I, 1959BOTT....2I...3C) U = Usher and collaborators (1981ApJS...46..117U, 1982ApJS...48...51U, 1982ApJS...49...27U, 1984ApJS...56..393H) K = Kiso UV survey PB = Palomar-Berger (1977A&AS...28..123B) L,LB = Luyten lists (Univ. Minnesota) G,GD = Giclas Proper Motion Survey (see cats. <I/79>, <I/112>) F = Feige (1958ApJ...128..267F) HZ = Humason-Zwicky (1947ApJ...105...85H) C,CB = Pesch & Sandyuleak (1983ApJS...51..171P, 1984ApJS...55..517S) --- Class Spectral classification --- Note a high dispersion spectrum exists --- Bmag Photoelectic Johnson's magnitude mag u_Bmag Uncertainty flag (:) on Bmag --- U-B Photoelectic Johnson's colour index mag u_U-B Uncertainty flag (:) on U-B --- B-V Photoelectic Johnson's colour index mag vmag Palomar photometric index number=4 Palomar 5m multichannel spectrophotometric indices defined by Greenstein (1976ApJ...207L.119G) centered at u=2.80um-1, g=2.12um-1, v=2.12um-1, r=1.44um-1 (wavenumbers micron-1) and calibrated in the AB79 system by Oke & Gunn (1983ApJ...266..713O) mag u_vmag Uncertainty flag (:) on vmag --- u-v Palomar photometric index number=4 Palomar 5m multichannel spectrophotometric indices defined by Greenstein (1976ApJ...207L.119G) centered at u=2.80um-1, g=2.12um-1, v=2.12um-1, r=1.44um-1 (wavenumbers micron-1) and calibrated in the AB79 system by Oke & Gunn (1983ApJ...266..713O) mag u_u-v Uncertainty flag (:) on u-v --- b-v Palomar photometric index number=4 Palomar 5m multichannel spectrophotometric indices defined by Greenstein (1976ApJ...207L.119G) centered at u=2.80um-1, g=2.12um-1, v=2.12um-1, r=1.44um-1 (wavenumbers micron-1) and calibrated in the AB79 system by Oke & Gunn (1983ApJ...266..713O) mag g-r Palomar photometric index number=4 Palomar 5m multichannel spectrophotometric indices defined by Greenstein (1976ApJ...207L.119G) centered at u=2.80um-1, g=2.12um-1, v=2.12um-1, r=1.44um-1 (wavenumbers micron-1) and calibrated in the AB79 system by Oke & Gunn (1983ApJ...266..713O) mag % Unexplained number --- Vmag V magnitude in Stroemgren system number=5 See a description of Stroemgren system in Geneva General Catalog of Photometric Data <GCPD/04> mag b-y Colour in Stroemgren system number=5 See a description of Stroemgren system in Geneva General Catalog of Photometric Data <GCPD/04> mag u_b-y Uncertainty flag (:) on b-y --- u-b Colour in Stroemgren system number=5 See a description of Stroemgren system in Geneva General Catalog of Photometric Data <GCPD/04> mag u_u-b Uncertainty flag (:) on u-b --- m1 Index (v-b)-(b-y) in Stroemgren system number=5 See a description of Stroemgren system in Geneva General Catalog of Photometric Data <GCPD/04> mag Refs References number=6 The values without citations are based on the authors' measurements. Otherwise the numbers refer to the following papers: 1 = Green =1980ApJ...238..685G 2 = Graham =1972AJ.....77..144G 3 = Greenstein =1984ApJ...276..602G 4 = Wegner =1983AJ.....88..109W 5 = Liebert & Stockman =1980PASP...92..657L 6 = Wesemael et al. =1985ApJS...58..379W 7 = Bond et al. =1984ApJ...279..751B 8 = Ferguson et al. =1981ApJ...251..205F 9 = Margon et al. =1981Natur.293..200M 10 = Ferguson et al. =1984ApJ...287..320F 11 = Green et al. =1982PASP...94..560G 12 = Becker et al. =1982MNRAS.201..265B 13 = Penning et al. =1984ApJ...276..233P 14 = Liebert et al. =1982ApJ...256..594L 15 = Liebert et al. =1984ApJ...277..692L 16 = Liebert et al. =1983ApJ...264..262L 17 = Barker & Cudworth =1984ApJ...278..610B 18 = Schmidt & Green =1983ApJ...269..352S 19 = Weymann et al. =1980Natur.285...64W 20 = Ellis et al. =1984PASP...96..283E 21 = Sion et al. =1985ApJ...292..477S 22 = Sion et al. =1985ApJ...292..471S 23 = Szkody et al. =1985ApJ...293..321S 24 = McGraw et al. =1979IAUCo..53..377M 25 = Winget et al. =1984IAUC.3932.....W 26 = Winget et al. =1984ApJ...279L..15W 27 = Nather et al. =1984IAUC.4021.....N 28 = Green =1976PASP...88..665G --- Heinz Andernach IUE/Vilspa Francois Ochsenbein CDS 1996 Sep 26 Thanks to Richard Green <green@noao.edu> for supplying an electronic version of his catalogue to H. Andernach <hja@vilspa.esa.es> in March 1994 UNKNOWN UNKNOWN * 17-Oct-1997: for PG 1535+547, in column "Comment", the cross- identification I Zw 120 chaged to I Zw 121 (H. Andernach) UNKNOWN UNKNOWN Nomenclature Notes: PG : the name is based on 1950 position. The first list of PG objects was presented by Green R.F., Greenstein J.L., and Boksenberg A. (1976PASP...88..598G) II_207.xml BVRI CCD photometry of 361281 objects in the field of M 31 2208 II/208 BVRI CCD photometry in the field of M 31 BVRI CCD photometry of 361281 objects in the field of M 31 E A Magnier W H G Lewin J van Paradijs G Hasinger A Jain W Pietsch J Truemper Astron. Astrophys. Suppl. Ser. 96 379 1992 1992A&AS...96..379M BVRI CCD photometry of 361281 objects in the field of M 31 E A Magnier W H G Lewin J van Paradijs G Hasinger W Pietsch J Truemper Astron. Astrophys. 272 695 1993 1993A&A...272..695M BVRI CCD photometry of 361281 objects in the field of M 31 Z Haiman E Magnier W H G Lewin R R Lester J van Paradijs G Hasinger W Pietsch R Supper J Truemper Astron. Astrophys. 286 725 1994 1994A&A...286..725H Photometry, CCD Regional catalog Stars, faint galaxies: individual (M 31) galaxies: photometry galaxies: spiral galaxies: stellar content Deep BVRI CCD photometry was performed on a 1 square degree region of M31. The observations were made between September 12 and September 27, 1990, using the McGraw-Hill 1.3m telescope at the Michigan-Dartmouth-MIT (MDM) observatory at Kitt Peak. The catalogue has typical completion limits of 22.3Bmag, 22.2Vmag, 22.2Rmag and 20.9Imag. Photometric accuracy is about 2% at Vmag=19. The final astrometric calibrations take into account the systematic error discovered in the Berkhuijsen etal (1987) catalog (Magnier etal 1993). They are in the J2000 system and are eventually tied to the HST Guide Star Catalog. The final photometric calibrations are tied via the NGC 206 region to photometry taken at the Michigan-Dartmouth-MIT (MDM) 1.3m in September and October 1993. These are tied to the Landolt (1992) system of standard stars, and are in the Johnson-Kron-Cousins system (BVRcIc). Caveats: There are several known problems with the catalog. First, there are likely to be some repeated detections of certain sources (i.e., multiple entries for the same object). Second, the wings of bright sources in some cases may be included as distinct sources. Third, the completeness limits are a strong function of position, and a much lower near the core and the core of M32. Fourth, variable stars, blended star, and stars with cosmic ray hits, cosmetic problems or other failures may have highly abnormal colors and magnitudes. In general, we expect these problems to be small, but the user is cautioned to watch for these possible problems.
Stars with both B and V photometry Stars with all B, V and I photometry The catalogue of M31 stars. Seq Sequence number --- RAdeg Right ascension (J2000) deg e_RAdeg Scatter for the star, if multiple measurements deg DEdeg Declination (J2000) deg e_DEdeg Scatter if multiple measurements deg Bmag =-9.999 B magnitude mag e_Bmag Mean error on Bmag mag o_Bmag Number of detection in B images number=2 negative numbers indicate that the object lies in a crowded area, and is likely to be either a blended image of two stars, or may be mismatched in the other filters. --- tBmag DoPHOT type for each detection number=1 See Schechter et al. (1993) for a description of DoPHOT; the "DoPHOT types" assign numbers depending of the similarity of the objects profile to the PSF. The definitions are: 1 = star 2 = extended profile (ie, galaxy) 3 = double profile (pair of stars) 4 = failed to converge in 4 parameter fit 5 = large number of bad pixels (ie, near the edge of CCD) 7 = failed to converge in 7 parameter fit. --- Vmag =-9.999 V magnitude mag e_Vmag Mean error on Vmag mag o_Vmag Number of detection in V images number=2 negative numbers indicate that the object lies in a crowded area, and is likely to be either a blended image of two stars, or may be mismatched in the other filters. --- tVmag DoPHOT type for each detection number=1 See Schechter et al. (1993) for a description of DoPHOT; the "DoPHOT types" assign numbers depending of the similarity of the objects profile to the PSF. The definitions are: 1 = star 2 = extended profile (ie, galaxy) 3 = double profile (pair of stars) 4 = failed to converge in 4 parameter fit 5 = large number of bad pixels (ie, near the edge of CCD) 7 = failed to converge in 7 parameter fit. --- Rmag =-9.999 R magnitude (Cousins) mag e_Rmag Mean error on Rmag mag o_Rmag Number of detection in R images number=2 negative numbers indicate that the object lies in a crowded area, and is likely to be either a blended image of two stars, or may be mismatched in the other filters. --- tRmag DoPHOT type for each detection number=1 See Schechter et al. (1993) for a description of DoPHOT; the "DoPHOT types" assign numbers depending of the similarity of the objects profile to the PSF. The definitions are: 1 = star 2 = extended profile (ie, galaxy) 3 = double profile (pair of stars) 4 = failed to converge in 4 parameter fit 5 = large number of bad pixels (ie, near the edge of CCD) 7 = failed to converge in 7 parameter fit. --- Imag =-9.999 I magnitude (Cousins) mag e_Imag Mean error on Imag mag o_Imag Number of detection in I images number=2 negative numbers indicate that the object lies in a crowded area, and is likely to be either a blended image of two stars, or may be mismatched in the other filters. --- tImag DoPHOT type for each detection number=1 See Schechter et al. (1993) for a description of DoPHOT; the "DoPHOT types" assign numbers depending of the similarity of the objects profile to the PSF. The definitions are: 1 = star 2 = extended profile (ie, galaxy) 3 = double profile (pair of stars) 4 = failed to converge in 4 parameter fit 5 = large number of bad pixels (ie, near the edge of CCD) 7 = failed to converge in 7 parameter fit. --- Francois Ochsenbein CDS 1996 Sep 06 It is a pleasure to thank Eugene Magnier <gene@astro.washington.edu> for providing the catalogue. II_208.xml An imaging K-band survey- I. The catalogue, star and galaxy counts. 2211 II/211 K-band survey in high galactic latitude An imaging K-band survey- I. The catalogue, star and galaxy counts. K Glazebrook J A Peacock C A Collins L Miller Mon. Not. R. Astron. Soc. 266 65 1994 1994MNRAS.266...65G An imaging K-band survey- I. The catalogue, star and galaxy counts. K Glazebrook J A Peacock L Miller C A Collins Mon. Not. R. Astron. Soc. 275 169 1995 1995MNRAS.275..169G Photometry, CCD Photometry, infrared Surveys Redshifts surveys stars: low-mass, brown dwarfs galaxies: evolution infrared: general The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R<19), long and multi-slit spectrographs for fainter objects.
Centres of IRCAM frames (table 2 of Paper I) RAh Right Ascension 1950 (hours) of centre h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) of centre --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec ExpTime Exposure time s fieldID Reference Star identifications --- The Survey (table 4 of Paper I) RAh Right Ascension 1950 (hours) of object h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) of object deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec [GPC94] Identification of the object --- Kmag Magnitude in K-band (2.2um) mag e_Kmag Mean error on Kmag mag Rmag Magnitude in R-band (red) mag n_Rmag 's' for saturated Rmag --- e_Rmag Mean error on Rmag mag Bmag Magnitude in B-band (blue) mag n_Bmag 's' for saturated Bmag --- e_Bmag Mean error on Bmag mag Vmag Magnitude in V-band mag n_Vmag 's' for saturated Vmag --- e_Vmag Mean error on Vmag mag Imag Magnitude in I-band (0.87um) mag n_Imag 's' for saturated Imag --- e_Imag Mean error on Imag mag Gflag Selection as a Galaxy --- Rflag Selectrion as a Reference --- fieldID Field ID number, as in table2. --- The spectroscopic sample (Table A1 of paper II) [GPC94] Identification as in table4 --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec z Redshift --- Ty Spectral type number=1 E = emission, predominantly [OII], H-beta and [OIII] A = absorption features (H+K, G, H{beta} to H{theta}) ER = strong H{alpha} emission --- K(4arcsec) Magnitude within 4arcsec aperture mag e_K(4arcsec) Mean error on K(4arcsec) mag K(20kpc) Magnitude within 20Mpc (Ho=100km/s/Mpc) mag e_K(20kpc) Mean error on K(20kpc) mag R(4arcsec) Magnitude within 4arcsec aperture mag e_R(4arcsec) Mean error on R(4arcsec) mag R(20kpc) Magnitude within 20Mpc (Ho=100km/s/Mpc) mag e_R(20kpc) Mean error on R(20kpc) mag w(K) Weight for incompleteness --- w(R) Weight for incompleteness --- Francois Ochsenbein CDS 1996 Oct 24 It is a pleasure to thank Karl Glazebrook <kgb@mail.ast.cam.ac.uk> for providing the electronic data, and Heinz Andernach <hja@vilspa.esa.es> for reformatting the data. II_211.xml A Finding List of Faint UV-Bright Stars in the Galactic Plane 2212A II/212A A Finding List of Faint UV-Bright Stars A Finding List of Faint UV-Bright Stars in the Galactic Plane H H Lanning Publ. Astron. Soc. Pac. 85 70 1973 1973PASP...85...70L A Finding List of Faint UV-Bright Stars in the Galactic Plane H H Lanning M Meakes Publ. Astron. Soc. Pac. 106 38 1994 1994PASP..106...38L A Finding List of Faint UV-Bright Stars in the Galactic Plane H H Lanning M Meakes Publ. Astron. Soc. Pac. 107 751 1995 1995PASP..107..751L A Finding List of Faint UV-Bright Stars in the Galactic Plane H H Lanning M Meakes Publ. Astron. Soc. Pac. 110 586 1998 1998PASP..110..586L Galactic plane Photometry, UBV Surveys Ultraviolet 195 UV-bright stars have been found on two-color 48-inch Schmidt plates centered on the galactic plane, and on one high-latitude plate. This catalog contains sources with (U-B) in the range U-B=0 to U-B=-1.5.
The Sandage two-color photographic survey was originally made in support of the UHURU x-ray satellite in order to identify those optical counterparts of the detected x-ray sources found in the galactic plane. During inspection of the plates, however, many UV-bright objects fainter than 10th magnitude were seen in the general field. A larger image in the U filter suggested the possibility of a bluer object as in the case of low-luminosity stars, white dwarfs, novae, CVs, normal early B stars, etc. As these are interesting in themselves, it was decided to publish a catalog for the use of other observers. This multi-color photographic technique has been described, for example, by Haro and Herbig (1955). The survey was concentrated on objects with m(B)~10 or fainter. It employed the Palomar 48-in (Oschin) Schmidt telescope and was centered on the galactic plane with overlapping regions covering the galactic latitudes +- 9 degrees, and extending throughout most of the northern plane (l = 0 deg - 227 deg). Plates were taken by J. Kristian, A.R. Sandage, R.J. Brucato, and Lanning, primarily. The data presented here were found following a careful examination of the plates but it should not be assumed these data represent a complete survey of the fields examined. The categories were roughly calibrated against photoelectric (U-B) measures, but a full scale calibration program, including magnitude effects, etc. was not done. The numerical (U-B) limits of the tables should not therefore be taken precisely. The blue magnitude of the sources in the finding list has been estimated using these photoelectric values as a guide but should be considered accurate to only +- 0.5 mag. due to the difficulty of adjusting to the various plate characteristics. Positions were measured from images retrieved from the Space Telescope Science Institute collection of Guide Star digital plate scans. The accuracy of positions from the Guide Star Catalog images has been estimated to be on the order of 0.2-0.8 arcsec (Russell et al. 1990) Information provided by Bidelman (private communication) resulted in the discovery that 15 positions for objects listed in Paper II were in error. Investigation indicated that an incorrect header was associated with the scan of the Guide Star plate originally archived onto optical disk. The incorrect astrometric solution, based on the use of an incorrect origin point, was subsequently applied in the positional determination when centroiding the object. The average offset for positions in right ascension is 14.17 seconds of time, with no detectable trend in the numbers. The offsets in declination range from +6.56 arcseconds through zero to -6.85 arcseconds as one progresses from west to east across the plate. This is consistent with a rotation being introduced into the bad plate solution. Objects with incorrect positions included Lanning 96, 97, 98, 99, 100, 102, 104, 108, 111, 113, 114, 115, 116, 119, and 122. uv.dat contains the corrected coordinates.
The stars with strong UV images ID Lanning number --- rem "*" indicates a note in notes.dat --- RAh Hours of Right Ascension (J2000) h RAm Minutes of Right Ascension (J2000) min RAs Seconds of Right Ascension (J2000) s DE- Sign of declination --- DEd Degrees of declination (J2000) deg DEm Minutes of declination (J2000) arcmin DEs Seconds of declination (J2000) arcsec Bmag Approximate blue magnitude mag u_Bmag : indicates B is uncertain --- U-B Approximate U-B mag u_U-B : indicates U-B is uncertain --- Notes on individual stars ID Lanning number The Lanning number is repeated when the text is longer than 75 characters. --- Text Text of Note --- N. G. Roman ADC/SSDOO 1997 Feb 10 The original author would like to thank Dr. R. J. Brucato for his assistance in the examination of some of the photographic plates for this two-color survey. Lanning and Meakes are very grateful to Dr. Peter Pesch for providing information regarding his unpublished observations of the high latitude sources noted in the text. They give special thanks to Dr. Allan Sandage for the opportunity to continue this survey. They also extend a special thanks to Dr. W. P. Bidelman who provided useful comments and information regarding the sources. They also greatly appreciate the ground-based observations taken by Dr. Alan Shafter (SDSU) and IUE data obtained by Dr. Al Schultz (CSC/STScI) in clarifying the classification of Lanning 185. The undersigned thanks Dr. Lanning for his help and particularly for a careful review of the finished files. UNKNOWN UNKNOWN * 10-Feb-1997: Papers I, II and III (Lanning numbers 1-195) * 07-Aug-1998: Paper IV appended (Lanning numbers 196-351) at CDS II_212A.xml The Optical Gravitational Lensing Experiment. The Catalog of Periodic Variable Stars in the Galactic Bulge. I. Periodic Variables in the Center of the Baade's Window 2213 II/213 OGLE Galactic Bulge periodic variables The Optical Gravitational Lensing Experiment. The Catalog of Periodic Variable Stars in the Galactic Bulge. I. Periodic Variables in the Center of the Baade's Window A Udalski M Kubiak M Szymanski J Kaluzny M Mateo W Krzeminski Acta Astron. 44 317 1994 1994AcA....44..317U The Optical Gravitational Lensing Experiment. The Catalog of Periodic Variable Stars in the Galactic Bulge. I. Periodic Variables in the Center of the Baade's Window A Udalski M Szymanski J Kaluzny M Kubiak M Mateo W Krzeminski Acta Astron. 45 1 1995 1995AcA....45....1U The Optical Gravitational Lensing Experiment. The Catalog of Periodic Variable Stars in the Galactic Bulge. I. Periodic Variables in the Center of the Baade's Window A Udalski A Olech M Szymanski J Kaluzny M Kubiak M Mateo W Krzeminski Acta Astron. 45 433 1995 1995AcA....45..433U The Optical Gravitational Lensing Experiment. The Catalog of Periodic Variable Stars in the Galactic Bulge. I. Periodic Variables in the Center of the Baade's Window A Udalski A Olech M Szymanski J Kaluzny M Kubiak M Mateo W Krzeminski K Z Stanek Acta Astron. 46 51 1996 1996AcA....46...51U The Optical Gravitational Lensing Experiment. The Catalog of Periodic Variable Stars in the Galactic Bulge. I. Periodic Variables in the Center of the Baade's Window A Udalski A Olech M Szymanski J Kaluzny M Kubiak M Mateo W Krzeminski K Z Stanek Acta Astron. 47.1 ??? ??? 1997 1997AcA....47....1U I/244 : OGLE General Catalog of stars. I. (Szymanski+ 1996) J/A+AS/125/343 : RR Lyr stars in omega Cen (Kaluzny+ 1997) ftp://sirius.astrouw.edu.pl/ogle : OGLE Internet Archive Stars, variable Photometry catalogs Stars: variables: general We present the Catalog of Periodic Variable Stars in the Galactic Bulge. The Catalog is based on observations collected during the OGLE (Optical Graviational Lensing Experiment) microlensing search: (1) 213 periodic variable stars brighter than Imag=18mag: 31 pulsating, 116 eclipsing and 66 miscellaneous type variables from the Baade's Window BWC field are presented. (2) 800 variable stars found in four Baade's Window fields BW1, BW2, BW3 and BW4 are presented. Among them 71 are classified as pulsating, 465 as eclipsing and 264 as miscellaneous type. (3) 644 variable stars: 64 pulsating, 352 eclipsing and 228 miscellaneous type were detected in four Baade's Window fields BW5, BW6, BW7 and BW8. Analysis of periodic variable stars found in overlapping regions of the Baade's Window fields yields an average completeness of the Catalog equal to about 80% of periodic variables objects registered in the OGLE databases and about 65% of all periodic variable stars in the observed region of the sky. (4) 631 variable stars: 59 pulsating, 348 eclipsing and 224 miscellaneous type were detected in third Baade's Window fields BW9, BW10, and BW11. (5) 574 variables stars: 44 pulsating, 369 eclipsing and 161 miscellaneous type were detected in four fields located symmetrically in the galactic latitude around the Galactic center: MM5-A, MM5-B, MM7-A and MM7-B.
Pulsating Variable Stars Eclipsing Variable Stars Miscellaneous Variable Stars OGLE OGLE star identification --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Per Period of pulsation d T0 Heliocentric Julian date of maximum brightness (minimum for eclipsing stars) d Imag I magnitude at maximum brightness mag V-I V-I colour index at maximum brightness mag DImag Imag amplitude mag Type Variability type --- Rem Remarks --- Patricia Bauer CDS 1997 Jul 09 UNKNOWN UNKNOWN Copied in April 1997 from ftp://sirius.astrouw.edu.pl/ogle/var_catalog II_213.xml The Combined General Catalogue of Variable Stars, 4.1 Edition. General Catalogue of Variable Stars 4th Edition, Volumes I-III, 2214A II/214A Combined General Catalogue of Variable Stars The Combined General Catalogue of Variable Stars, 4.1 Edition. General Catalogue of Variable Stars 4th Edition, Volumes I-III, P N Kholopov N N Samus M S Frolov V P Goranskij N A Gorynya E A Karitskaya E V Kazarovets N N Kireeva N P Kukarkina N E Kurochkin G I Medvedeva E N Pastukhova N B Perova A S Rastorguev S Yu Shugarov Moscow: Nauka Publishing House ??? ??? 1985-1988 The Combined General Catalogue of Variable Stars, 4.1 Edition. General Catalogue of Variable Stars 4th Edition, Volumes I-III, P N Kholopov N N Samus O V Durlevich E V Kazarovets N N Kireeva T M Tsvetkova Institute of Astronomy of Russian Academy of Sciences and Sternberg State Astronomical Institute of the Moscow State University, Nauka, Moscow, ??? ??? 1990 The Combined General Catalogue of Variable Stars, 4.1 Edition. General Catalogue of Variable Stars 4th Edition, Volumes I-III, N M Artiukhina O V Durlevich M S Frolov V P Goranskij N A Gorynya E A Karitskaya E V Kazarovets P N Kholopov N N Kireeva N E Kurochkin N A Lipunova G I Medvedeva E N Pastukhova N N Samus T M Tsvetkova "Kosmosinform", Moscow, ??? ??? 1995 The Combined General Catalogue of Variable Stars, 4.1 Edition. General Catalogue of Variable Stars 4th Edition, Volumes I-III, B V Kukarkin P N Kholopov N M Artiukhina V P Fedorovich M S Frolov V P Goranskij N A Gorynya E A Karitskaya N N Kireeva N P Kukarkina N E Kurochkin G I Medvedeva N B Perova G A Ponomareva N N Samus S Yu Shugarov Moscow: Nauka Publishing House ??? ??? 1982 II/195 : Namelists of variable stars II/219 : New Suspected Variable Stars Supplement (Kazarovets+ 1999) ftp://ftp.sai.msu.su/pub/groups/cluster/gcvs : Sternberg files http://www.sai.msu.su/groups/cluster/gcvs/gcvs/ : GCVS DatabaseAitken, R. G. 1932, "New General Catalogue of Double Stars within 120 Degrees of the North Pole", Carnegie Institution of Washington Pub. 417 (Washington, D.C.: Carnegie Institution of Washington). Argelander, F. 1859-62, "Bonner Sternverzeichnis. Erste bis dritte Sektion", Astronomischen Beobachtungen auf der Sternwarte der Koeniglichen Rhein. (Cat. <I/122>) Artiukhina N.M., Durlevich O.V., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kazarovets E.V., Kholopov P.N., Kireeva N.N., Kurochkin N.E., Lipunova N.A., Medvedeva G.I., Pastukhova E.N., Samus N.N., Tsvetkova T.M., 1995, General Catalogue of Variable Stars, 4rd ed., vol.V. Extragalactic Variable Stars, "Kosmosinform", Moscow Cannon, A. J. and Pickering, E. C. 1918-1924, "The Henry Draper Catalogue", Ann. Astron. Obs. Harvard College 91-99. (Cat. <III/135>) Dreyer, J. L. E. 1888, "New General Catalogue of Nebulae and Clusters of Stars", Mem. Roy. Astron. Soc. 49, Part I (reprinted 1962, London: Royal Astronomical Society) (see Cat. <VII/1>) Durlevich O.V., Frolov M.S., Kazarovets E.V., Samus N.N, 1996, Bull. Inf. CDS 48, 35 Durlevich O.V., Frolov M.S., Kazarovets E.V., Samus N.N., 1994, The list of errors in the GCVS, 4th edition. I. Volumes I-III, Bull. Inf. CDS, 45, 19 Gill, D. and Kapteyn, J. C. 1895-1900, "Cape Photographic Durchmusterung, Ann. Cape Obs." 3 (1895, Part I: zones -18 to -37); 4 (1897, Part II: zones -38 to -52); 5 (1900, Part III: zones -53 to -89; Cat. <I/108>). Hoffleit, D. (with the collaboration of Jaschek, C.) 1982, "The Bright Star Catalogue" (New Haven: Yale University Observatory; see Cat. <V/50>). Kazarovets E.V., Samus N.N., Goranskij V.P., 1993IBVS.3840....1K Kazarovets E.V., Samus N.N., 1995IBVS.4140....1K Kholopov P.N., Samus N.N., Durlevich O.V., Kazarovets E.V., Kireeva N.N., Tsvetkova T.M., 1990, General Catalogue of Variable Stars, 4rd ed., vol.IV(Moscow, Nauka Publishing House, Cat. <II/205>) Kholopov P.N., Samus N.N., Durlevich O.V., Kazarovets E.V., Kireeva N.N., Tsvetkova T.M., 1992, Bull. Inf. CDS, 40, 15. Kholopov P.N., Samus N.N., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kazarovets E.V., Kireeva N.N., Kukarkina N.P., Kurochkin N.E., Medvedeva G.I., Pastukhova E.N., Perova N.B., Rastorguev A.S., Shugarov S.Yu., 1985 -- 1988, General Catalogue of Variable Stars, 4rd ed., vols. I -- III, Nauka, Moscow; Cat. <II/139>. Kuestner, F. 1903, "Bonner Durchmusterung des Noerdlichen Himmels, zweite berichtigte Auflage", Bonn Universitats Sternwarte. (Cat. <I/122>) New Catalogue of Suspected Variable Stars, Kukarkin B.V., Kholopov P.N., Artiukhina N.M., Fedorovich V.P., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kireeva N.N., Kukarkina N.P., Kurochkin N.E., Medvedeva G.I., Perova N.B., Ponomareva G.A., Samus N.N., and Shugarov S.Yu. 1982, Moscow: Nauka Publishing House Office. (Cat. <II/140>) Kukarkin, B. V., Kholopov, P. N., Efremov, Yu. N., and Kurochkin, N. E. 1965, "Second Catalogue of Stars Suspected of Variability" (Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.). Kukarkin, B. V., Parenago, P. P., Efremov, Yu. N., and Kholopov, P. N. 1951, "Catalogue of Stars Suspected of Variability" (Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.). Neugebauer, G. and Leighton, R. B. 1969, "Two-Micron Sky Survey, A Preliminary Catalog", NASA SP-3047 (Washington, D.C.: National Aeronautics and Space Administration; cat. <II/2>). Parenago, P. P. 1954, Trudy Sternberg Astron. Inst. No. 25. Prager, R. 1934, Ergaenz. Astron. Nachr. 9, No. 3. Prager, R. 1937, Ergaenz. Astron. Nachr. 10, No. 1. Schoenfeld, E. 1886, "Bonner Sternverzeichniss" , Vierte Sektion, Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rheinischen Friedrich-Wilhelms-Universitat zu Bonn 8, Part IV (Bonn: Adolph Marcus; cat. <I/119>). Smithsonian Astrophysical Observatory Staff 1966, "Star Catalog. Positions and Proper Motions of 258,997 Stars for the Epoch and Equinox of 1950.0", Publ. of the Smithsonian Institution of Washington, D.C., No. 4652 (Washington: Smithsonian Institution); see cat. <I/131> Sulentic, J. W. and Tifft, W. G. 1973, "The Revised New General Catalogue of Nonstellar Astronomical Objects" (Tucson: The University of Arizona Press); cat. <VII/1>. Thome, J. M. 1892-1932, "Cordoba Durchmusterung, Resultados del Observatorio Nacional Argentino" 16 (1892, Part I: -22 to -32 Degrees), 17 (1894, Part II: -32 to -42 Degrees), 18 (1900, Part III: -42 to -52 Degrees), 21 (Part I) (1914, Part IV, -52 to -62 Degrees), 21 (Part II) (1932, Part V: -61 to -90 Degrees); cat. <I/114>. Warren, W.H., Jr. 1988, "New Catalogue of Suspected Variable Stars", Documentation for the Machine-Readable Version, NSSDC/WDC-A-R&S 88-24. Warren, W.H., Jr. 1989, "General Catalogue of Variable Stars", 4th edition, Documentation for the Machine-Readable Version, NSSDC/WDC-A-R&S 88-23 Zinner, E. 1929, Ergaenz. Astron. Nachr. 8, No. 1. Stars, variable Combined data Supernovae The GCVS is the only reference source on all known variable stars. This version contains all of the electronically-readable version as distributed by the Sternberg Astronomical Institute and Institute of Astronomy (Russian Acad.Sci.), Moscow. It includes the catalog of variable stars, updated and completed with the seven Name-Lists of Variables Stars Nos.67-73 (see IBVS No.2681,1985; No.3058,1987; No.3323,1989; No.3530,1990; No.3840,1993; No.4140,1995; No.4471,1997), a catalog of suspected variables, a cross-index of variable star names, a catalog of extragalactic variables, and a catalog of supernovae.
The present improved electronic version of the GCVS4 Volumes I-V, combined with Name-Lists of Variable Stars Nos.67-73, are also available from Sternberg Institute via anonymous ftp to ftp.sai.msu.su, /pub/groups/cluster/gcvs... and via http://www.sai.msu.su/groups/cluster/gcvs/ . The information at this site is regularly updated (corrections of detected mistakes, improvements of identifications and coordinates, etc.). gcvs.dat is the combined computer-readable version of the GCVS4 Vols. I-III (Kholopov et al. 1985-1988) and Name-Lists of Variable Stars Nos.67-73 (1985IBVS.2681....1K, 1987IBVS.3058....1K, 1989IBVS.3323....1K, 1990IBVS.3530....1K, 1993IBVS.3840....1K, 1995IBVS.4140....1K and 1997IBVS.4471....1K) published in the system introduced during the preparation of the 4th GCVS edition. The total number of designated variable stars has now reached 31918; of them, 3506 stars enter the Name-Lists Nos.67-73. Errors detected in the printed Volumes I-III and in the Name-Lists were corrected; the file includes also improved equatorial positions for some variable stars. crossid.dat contains all variables, including extragalactic variables, stars from the Name-Lists, and stars suspected of variability since the compilation of the NSV catalog, ordered by right ascension (B1950). The authors tried to provide as complete lists as possible for the stars identified with the catalogues HD, BD, CoD, CPD, BS, ADS and for the stars with preliminary HV (Harvard Variable) designations. As for the other catalogues, their task here was more difficult since they had to rely upon references to source catalogue names made by variable star researchers; the tables in the present volume reproduce the materials used in their work, and incompleteness seems to be unavoidable. Starting with Name-List No.71, the identifications became more reliable and complete thanks to special effort of the compilers. The final, fifth volume contains data for variables in external galaxies (including the Magellanic Clouds) and for extragalactic supernovae (see evs*.dat and sn*.dat). All variables in the present data set are arranged in the order of their names inside constellations. For Name-list stars, the information follows the format of the Name-Lists, that is, it includes only coordinates, the variability type, the range of brightness variations, and references. The file nsv.dat is a compilation of 14811 stars suspected of variability and not finally designated as variables prior to 1980. It is the successor to the "Catalogues of Stars Suspected of Variability" published in 1951 and 1965 (Kukarkin et al.). Data contained in the present catalog include positions, magnitudes, variability types, alternate designations, and references to the literature. The computer version of NSV contains principally the same data as in the printed catalog, but only the data table without the textual material (bibliography, remarks) is included. Necessary corrections were introduced, as of June, 1997, and coordinates were improved, compared to the printed version, for about half of the stars in the catalog. The Sternberg Institute has started preparation of an electronic release GCVS 4.2 which will contain improved light elements, classifications etc. along with sufficiently accurate positional information. The first approach to this project has resulted in improved equatorial positions (B1950, J2000) for variable stars in the constellations of Andromeda, Antlia and Apus including the stars from the GCVS proper plus the stars from the subsequent Name-lists, with a new standard of positional accuracy, to 1 second of arc (IAU Inform. Bull. Var. Stars, in preparation). These positions have been incorporated in the present data set.
Combined GCVS (vols I-III and name lists) Constell Constellation numeric code --- Number Star number within the constellation --- Component Component identification designations of components of double/multiple stars: A,B; 1,2,3 ... (tau 1). Usually only one component of the binary is variable, but there exist two cases (CE Cas A,B; EQ Peg A,B) when both components are variable and enter the catalogue as separate lines. --- GCVS Variable star designation traditional transliterations of greek letters are used. Lower- and upper-case latin letters must be distinguished (e.g. u Her and U Her). --- NoteFlag Notes in published catalog see the document by Kholopov et al. (1985-1988). --- RAh Hours RA, equinox 1950.0 the position is not listed when the variable is equivalent to another catalogued variable ("=" in column Exists, byte 142). h RAm Minutes RA, equinox 1950.0 min RAs Seconds RA, equinox 1950.0 s DE- Sign Dec, equinox 1950.0 --- DEd Degrees Dec, equinox 1950.0 deg DEm Minutes Dec, equinox 1950.0 arcmin DEs Seconds Dec, equinox 1950.0 arcsec u_DEs position accuracy flags the real coordinates accuracy uses the symbols: (:) means right ascensions accurate to one second of time and declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. (') means right ascensions accurate to one minute of time and declinations accurate to one arcminute. --- VarType Type of variability type of variability. The system of variable star classification corresponds to the GCVS4, with six additions (ZZO, AM, R, BE, LBV, BLBOO) introduced in the Name-Lists 67- 72 and in the GCVS vol.V (see file "vartype.txt"). --- l_magMax ">" if magMax is a faint limit "<" if magMax is a bright limit "(" if magMax is an amplitude --- magMax Magnitude at maximum brightness mag u_magMax Uncertainty flag (:) on magMax --- f_magMax ")" if magMax is an amplitude --- l_magMin "<" if magMin is a bright limit "(" if magMin is an amplitude --- magMin Minimum magnitude or amplitude mag u_magMin Uncertainty flag (:) on magMin --- n_magMin Alternative photometric system for magMin Code for alternative photometric system. Field is non-blank if magMin is a magnitude or amplitude given in a system other than that indicated by magCode. An asterisk in the corresponding position means the amplitude measured in white light. --- f_magMin ")" if magMin is an amplitude --- magCode The photometric system for magnitudes the photometric system in which magMin and magMax are reported (see also Note on n_magMax, n_magMin). The main codes are P (photographic magnitudes) and V (visual, photovisual, or Johnson's V). See also the documents by Kholopov et al. (1985-1988) or Warren (1989). Several stars from the 68th Name-List have in these positions "1." designating the 1.04 micrometer band of the system introduced by G.W.Lockwood. The designations u,v,b,y refer to the Stroemgren system. The symbols "I" and "R" mean magnitudes in Cousins' I system. "g" designates magnitudes in the system of Thuan and Gunn; "T" stands for broad-band Tycho magnitudes formed from B and V measurements; "r" are red magnitudes not tied to a particular system. --- Epoch Epoch for maximum light, Julian days Epochs are given for minimum light for all eclipsing and ellipsoidal variables, as well as for RV Tau and RS CVn types, and for maximum for all other types. This rule may occasionally be broken, but this is explained only in the remarks to the catalog, which are not available in machine-readable form at this time. The epochs are Julian dates. For novae (types N) and supernovae (types SN), the Epoch is completed by a year of outburst in the YearNova column. d q_Epoch Quality flag on Epoch the following codes are used (see also note on Epoch) : ":" epoch is uncertain. "+" epoch may be later than that reported; "-" epoch may be earlier than that reported. --- YearNova Year of outburst for nova --- l_Period Code for upper or lower limits the following codes are used: ">" or "<" if period is a lower or upper limit, respectively. "(": the period is the mean cycle time of a U Gem or recurrent nova (in this case, there is ")" in n_Period column) --- Period Period of the variable star d u_Period Uncertainty flag (:) on Period --- n_Period Uncertainty notes on Period the following codes are used: "*N" if the period may be a multiple of the quoted value; "/N" if the period may be a fraction of the quoted value; ")" - see the note on l_Period. --- M-m/D Rising time (M-m) or duration of eclipse (D) this column holds the rising time (M-m) of intrinsic variables, or the duration of the eclipse (D) for eclipsing binaries. These values help to define the shape of the light curve. The value is given in percentage of the period of the star. % u_M-m/D Uncertainty flag (:) on M-m/D --- n_M-m/D Note for eclipsing variable the "*" indicates that the duration of the light constancy phase at minimum light (d) for an eclipsing variable is equal to zero. --- SpType Spectral type --- Ref1 Reference to a study of the star "00001" - if the main characteristics of the star were determined by the authors themselves. "00002" - "09148" - Vol. I GCVS (see Kholopov et al., 1985-1988). "09149" - "09558" - Vol. II GCVS "09559" - "10200" - Vol. III GCVS "V 001" - "V 554" - Vol. V GCVS (see file evs_ref.dat) "67001" - "73381" - Name-Lists Nos.67-73 (see file nl_ref.dat) If no chart is available for the variable, but the star is contained in one of the Durchmusterung catalogs or the Hubble Space Telescope Guide Star Catalog, the corresponding abbreviation (BD, CPD, CoD, GSC) is given. --- Ref2 Reference to a chart or photograph --- Exists Cases of non-existence of the variable etc. the following codes are used in column Exists: "N" in byte 142 if the star does not exist. "=" in byte 142 appears in three cases. First, it is used if the variable is equivalent to another catalogued variable. In such case, after the "=" symbol, the alternative name of the variable follows, and all necessary information on the star is to be found under that alternative name. Second, it is used for all variables of the Name-Lists Nos.67-73, it is followed by the two-digit number of the Name-list and the four-digit number of the star in the Name-list, and the information for the star follows the format of the Name-lists (see above). Third, the "=" symbol may be followed by the star's name in the GCVS Vol. V (see the file evs_cat.dat). This means that the star enters also Vol. V, and the information of Vol. V makes it possible to improve the data of Vols. I-III. In this case, the symbol "*" in byte 153 means the presence of remarks in Vol. V; the symbol(s) "n" or "n:" in bytes 154-155 means that the star is nonmember (possible nonmember) of the galaxy in question. --- RA2000h Hours RA, equinox 2000.0 h RA2000m Minutes RA, equinox 2000.0 min RA2000s Seconds RA, equinox 2000.0 s DE2000- Sign Dec, equinox 2000.0 --- DE2000d Degrees Dec, equinox 2000.0 deg DE2000m Minutes Dec, equinox 2000.0 arcmin DE2000s Seconds Dec, equinox 2000.0 arcsec *The Cross-Identifications of Variable Stars Cat Abbreviated name of catalog or list -------------------------------------------------------------------- ADS = R.G.Aitken, 'New General Catalouge of Double Stars', Carnegie Inst. of Washington Publ. no.417, vols.I, II, 1932 AN = Preliminary designations of variable stars introduced by the 'Astronomische Nachrichten' AS = P.W. Merrill, C.G.Burwell, 'Additional Stars whose Spectra have a Bright H Alpha Line', Astrophys. J. 112, 72, 1950 (=1950ApJ...112...72M); see also Astrophys. J. 113, 624, 1951 (=1951ApJ...113..624M) BAY = Bayer, list of those bright stars having designations by Greek letters in their constellations BD = Bonner Durchmusterung, F.W.A. Argelander, Bonner Sternverzeichniss, 1 bis 4 sektion, Astronomische Beobachtungen auf der Sternwarte de Kgl. Rhein/ Friedrich-Wilhelms-Unviersiaet zu Bonn (Catalogs <I/119> and <I/122>) BS (HR) = D. Hoffleit, 'The Bright Star Catalogue', 4th Revised Ed., Yale University Observatory, New Haven, Conn. USA, 1982 (see catalog <V/50>) CoD = Cordoba Durchmusterung, J. M. Thome, Resultados del Observatorio Nacional Argentino 16 - 18; 21, 1892-1932 (catalog <I/114>) CPD = Cape Photographic Durchmusterung, D. GIll and J. C. Kapteyn, Ann. Cape Obs. 3-5, 1895 - 1900 (catalog <I/108>) CRL (AFGL) = Air Force Geophysics Laboratory. Four-Color Infrared Sky Survey (and supplement): S.D. Price and R.G. Walker - AFGL-TR-76-028 (Hanscom AFB, MA, Air Force Geophysics Lab., Air Force Systems Command, USAF, 1976; S.D. Price and T.L. Murdock - Air Force Geophysics Laboratory, AFGL-TR-83-0161 (see catalog <II/94>) EG = O.J. Eggen, J.L. Greenstein, 'Spectra, Colors, Luminosities, and Motions of the White Dwarfs', Astrophys. J. 141, 83 (1965ApJ...141...83E); additional stars in Astrophys. J. 142, 925 (1965ApJ...142..925E) and 150, 927 (1967ApJ...150..927E); more stars added by J.L. Greenstein, see references in McCook and Sion, Astrophys. J. Suppl. 65, 603 (1987ApJS...65..603M) FLM = Flamsteed, List of those bright stars having designations by number in their constellations G = H.L. Giclas, R. Burnham Jr., and N.G. Thomas, (Large Proper Motion Stars) - Publications of Lowell Obs., Flagstaff, Arizona, 1971 (Catalogs <I/79> and <I/112>) GD = H.L. Giclas White Dwarfs (Lowell Obs.) Gl = W. Gliese, 'Catalogue of Nearby Stars', Veroeff. Astron. Rechen-Inst. Heidelberg nr.22, 1969; W. Gliese, H. Jahreiss, 'Nearby star data published 1969-1978', Astron. Astrophys. Suppl. 38, 423 (1979A&AS...38..423G); see catalog <V/70> HD = Henry Draper Catalogue - A.J. Cannon and E.C. Pickering, Havard Obs. Ann. 91 - 99, 1918-1924; A. J. Cannon, Harvard Obs. Ann. 100, 1925 - 1936; see catalog <III/135> He = A number of lists of planetary nebulae and emission-line stars by K. Henize HII = E. Hertzsprung, 'Catalogue de 3259 Etoiles dans les Pleiades', Ann. Sterrewacht Leiden, 19, pt. 1A, 1947 HRC = G.H. Herbig, N.K. Rao, 'Second Catalog of Emission-line Stars of the Orion Population', Astrophys. J. 174, 401 (1972ApJ...174..401H); G.H. Herbig, K.R. Bell, 'Third Catalog of Emission-Line Stars of the Orion Population', Lick Obs. Bull. no. 1111, 1988 (catalog <V/73>) HV = Harvard variables IRC = G. Neugebauer, R.B. Leighton, 'Two-Micron Sky Survey, A Preliminary Catalog', NASA SP-3047, 1969; catalog <II/2> LH = Lick H Alpha: A number of lists of emission-line stars by G.H. Herbig MH = Mount Wilson H-Alpha Stars, see references for MWC and AS MWC = P.W. Merrill, C.G. Burwell, 'Catalogue and Bibliography of Stars of Classes B and A Whose Spectra have Bright Hydrogen Lines', Astrophys. J. 78, 87 (1933ApJ....78...87M) (Mount Wilson Catalogue); Supplements: Astrophys. J. 98, 153 (1943ApJ....98..153M); 110, 387 (1949ApJ...110..387M) OH = OH sources designated by their galactic coordinates Par = A List of Stars in the Region of the Orion Nebula (P.P. Parenago, Sternberg Inst. Publ. vol. 25, 1954; catalog <II/171>) PG = Palomar-Green survey S = Preliminary designations of variables discovered at Sonneberg Observatory SAO = 'Smithsonian Astrophysical Observatory Star Catalog', parts I-IV, Smithsonian Inst. Washington, 1966 (catalog <I/131>) SVS = Soviet Variable Stars (preliminary designations of Soviet-discovered variables) VV = Vatican variable stars WD = G.P. Mc Cook, E.M. Sion, 'Catalog of Spectroscopically Identified White Dwarfs', Astrophys. J. Suppl. 65, 603 (1987ApJS...65..603M); see catalog <III/129>. WR = K.A. van der Hucht et al. 'The Sixth Catalogue of Galactic Wolf-Rayet Stars, Their Past and Present', Space Sci. Rev. 28, 227, 1981 (Catalog <III/85>) --- Seq Star number or name in the respective catalog --- m_Seq Component designation Designations of components of double/multiple stars: A,B,C ...; a,b,c ...; 1,2,3 ...; the symbols P = preceding, F = following, N = northern, S = southern may also appear. In the cases of ADS 03201 and ADS 03202 the symbols k1 and k2 mean kappa 1 and kappa 2, respectively. --- Vname Designation in GCVS or NSV name of the object in the GCVS, its Volume V, or the NSV. Lower- and upper-case latin letters must be distinguished (e.g. u Her and U Her). --- m_var Component designation --- IDflag Uncertainty flag on cross-identification. --- Extragalactic Variable Stars. Catalogue GalNo Galaxy code Code identifying the galaxy. This numbering system begins with 089, the first 88 codes being reserved for constellations (cf. catalog <II/139>). Note that NGC 1466 is a globular cluster (not a galaxy) between the LMC and the SMC; we presented it separately, because it is not clear to which galaxy to attribute its variable stars. --- VarNo Variable star number within the galaxy variable star No within the galaxy. Number of the variable star in the galaxy. If in the literature for the considered galaxy there exist several different variable star numbering systems, we have introduced new numbers in the order of increasing right ascension for the equinox 1950.0. But if the variable star numbering system for the galaxy is practically of general use, we have retained it - if necessary, with additional numbers ordered by increasing right ascension. --- Name Variable star designation Variable star Designation. The name of the variable in the adopted system of variable star designations: name of the galaxy + "V" + variable star No. within the galaxy (see column VarNo) --- RemFlag indicates a remark in file evs_rem.dat --- RAh Right ascension, equinox 1950.0 If the star's coordinates are only roughly known, they are nevertheless formally presented to one second of time in right ascension (with the decimal point following) and to one arcsecond in declination (with the decimal point following). See column u_DEs which indicates the real accuracy. h RAm (minutes) min RAs (seconds) s DE- sign of declination, 1950.0 --- DEd Declination, equinox 1950.0 deg DEm (arc minutes) arcmin DEs (arc seconds) arcsec u_DEs accuracy flags the real coordinates accuracy uses the symbols: (") means right ascensions accurate to one second of time and declinations accurate to one arcsecond; (:) means declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. (!) for V0474 in the Sculptor system, the listed coordinates refer to the galaxy's center since the coordinates of the star itself are unknown. --- VarType Type of variability type of variability. The classification systems corresponds to the GCVS vols. I-III (catalog <II/139>), with the addition of the new "BLBOO" type, called after the prototype star BL Boo = NGC 5466 V19 referring to the so-called "anomalous Cepheids", i.e. stars with periods characteristic of comparatively long-period RRAB variables, but considerably brighter by luminosity. There are also suspected variables designated by the symbol "var:". --- magMax Magnitude at maximum brightness mag u_magMax Uncertainty flag (:) on magMax --- l_magMin magMin is an upper limit or amplitude minMag contains the minimum brightness, or the variability amplitude instead (in brackets, i.e. l_magMin='(' and n_magMin=')'). (<) means that minMag is an upper limit (light) --- magMin Magnitude at minimum brightness, or amplitude mag u_magMin Uncertainty flag (:) on magMin --- n_magMin ")" if magMin is an amplitude --- magCode Code for photometric system designation of the photometric band. P means photographic magnitudes, V means visual or photovisual magnitudes as well as V system magnitudes. In the latter case, they are usually distinguishable from visual magnitudes by the number of digits after the decimal point (as a rule, V system magnitudes are based upon photoelectric or CCD photometry). Letters U, B, R, I, J, H, K, L, M, N, O, Q mean, as a rule, magnitudes expressed in corresponding systems of broad-band photometry. --- Epoch Epoch The epoch expressed as Julian Date. For eclipsing and ellipsoidal variables, RV Tau and RS CVn stars, the catalogue gives epochs of minimum light, and for the rest of variables, epoch of maximum light. For novae (types N) and supernovae (types SN), the Epoch is completed by a year of outburst (YearNova column). d u_Epoch Uncertainty flag on Epoch --- l_P '(' for U Gem For U Gem stars and recurrent novae, the P column gives (in brackets) the mean cycle value, if known. --- P Period d u_P Uncertainty flag (:) on P --- n_P ')' for U Gem --- M-m/D M-m or D Duration of light increase from minimum to maximum (M-m) for intrinsic variable stars or the eclipse duration (D) for Algol type variables are expressed in hundredths of the photometric period for the star in question. An asterisk (*) in n_M-m/D means, for an eclipsing variable, that the duration of the constant brightness phase in minimum (d) for this star is equal to zero. % u_M-m/D Uncertainty flag (:) on M-m/D --- n_M-m/D Note for eclipsing variable --- SpType Spectrum If there exist several spectral type determinations for a star, we preferred more recent ones, taking into account reliability of each determination. We converted symbols "d" (dwarfs) and "g" (giants) into luminosity classes V and III. If a nova showed spectral features typical of novae during or after the outburst, a symbol (NOVA) is given in this column. If the spectrum shows features characteristic of U Gem variables, this column contains the symbol (UG). Continuous spectrum is designated "cont", the symbol "e" means emission spectrum, lower case letters "ea", "eb" in this column stand for "e alpha", "e beta". For RR Lyrae stars, spectral types from hydrogen lines are given. A plus sign (+) between two spectral type values means that spectra of two components of a spectroscopic binary are observed. Two spectral type values separated with a minus sign (-) mean the range of spectral type variations in the process of brightness changes. --- evsRef1 Reference for study of the star, see file evs_ref.dat --- evsRef2 Reference for chart or photograph, see file evs_ref.dat --- Desig1 designation in paper Ref1 --- Desig2 designation in paper Ref2 --- VarName Designation in gcvs.dat or nsv.dat --- nonMem Non-member note Symbols "n" or "n:" for nonmembers (possible nonmembers) of the galaxy in question. For the stars that enter the GCVS vols. I-III (file gcvs.dat) or the NSV catalogue (file "nsv.dat") and are not members of the corresponding galaxy, the present volume gives only the running number, coordinates, the symbol "n", and the GCVS or NSV name. --- YearNova Year of outburst yr u_YearNova Uncertainty flag on YearNova --- Extragalactic Variable Stars. Remarks Name Variable star designation When more than one line is required, this field is repeated. --- Text Text of remark --- Extragalactic Variable Stars. References evsRef Reference number, repeated if more than 1 line --- --- Period ending number --- Text Text of reference --- Extragalactic supernovae. Catalogue SN Supernova designation --- n_SN Doubtful (?), or rejected (-) SN --- RemFlag The '*' indicates a remark in sn_rem.dat --- Gal Parent galaxy designation "N" means NGC catalogue numbers, "I" refers to the IC catalogue, "U" to the UGC catalogue, "M" to the MCG catalogue, "E" to ESO survey lists. "An" means an anonymous galaxy "Intergal" is for cases when the supernova cannot be reliably attributed to a particular galaxy and is considered intergalactic. --- RAh RA 1950 (hours) of Parent galaxy h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination Deg. 1950 of Parent galaxy deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec u_DEs Accuracy flags The real coordinates accuracy is denoted by (") means right ascensions accurate to one second of time and declinations accurate to one arcsecond; (:) means declinations accurate to one tenth of an arcminute; (') means declinations accurate to one arcminute. --- MType Type of the parent galaxy --- BT Integrated magnitude of parent galaxy mag u_BT Uncertainty flag (:) on BT --- n_BT Band indicator, blank for photographic --- maxDate Date of the SN's maximum or of discovery The date of the SN's maximum or of discovery, or of an isolated observation at high brightness. If maxDate or f_magMax contains an asterisk (*), it means that the date and/or the magnitude refer not to the maximum (not covered with observations), but to the EPOCH OF DISCOVERY or to an isolated observation at high brightness. As a rule, information about maxima was not included if it was based on considerable extrapolation. --- magMax Magnitude at maximum (light) of SN mag u_magMax Uncertainty flag (:) on magMax --- n_magMax Band indicator, blank for photographic --- f_magMax '*' if maximum not observed --- dRA Distance of SN from galaxy nucleus In line 393, 1970K, the offset is 0.3E arcsec oRA Orientation of dRA --- dDE Distance of SN from galaxy nucleus In line 732, 1988T, the offset is 0.4N arcsec oDE Orientation of dDE --- RASN.h Right Ascension 1950 (hours) of SN h RASN.m Right Ascension 1950 (minutes) min RASN.s Right Ascension 1950 (seconds) s DESN.- Declination 1950 (sign) --- DESN.d Declination 1950 (degrees) of SN deg DESN.m Declination 1950 (minutes) arcmin DESN.s Declination 1950 (seconds) arcsec u_DESN.s accuracy flags on SN position --- SNType SN classification Limited to types I (I-A, I-B) and II (II-l, II-pl), with possible indications of peculiarities (pec). --- Discov Name of the SN discoverer In case of several discoverers, the name of the first author of the discovery is given followed by "+" symbol. As a rule, information on independent rediscoveries is not presented in the remarks, for the sake of brevity. The abbreviation "BASST" in this column means that the supernova was discovered by the Berkeley Automated Supernova Search Team. --- snRef1 Reference for study of the star See file sn_ref.dat --- snRef2 Reference for chart or photograph --- Extragalactic supernovae. Remarks SN Supernova designation, repeated if more than 1 line --- n_SN Doubtful (?), or rejected (-) SN --- Text Text of remarks --- Extragalactic supernovae. References snRef Reference number, repeated if more than 1 line --- --- Period following Reference number --- Text Text of reference --- References for name lists NLnum Name-List number --- Ref Reference number In the present version the authors attempted to give Latin transliterations of Russian-language names of astronomical periodicals and books. They did not try to unify the Latin spelling of names with Cyrillic (or other) original forms, but simply tried to reproduce the Latin transcriptions in the publications referred to. Of course this may lead to some confusion, hopefully minor. If a paper enters lists of references of several Name-Lists, it appears several times in the present version. --- Text Text of reference --- *Suspected variables NSV NSV number --- NSVLetter NSV letter suffix The letter "A" is present for one star, NSV 10360A, which is a completely different object from NSV 10360. --- u_NSV Dubitancy flag if a star's variability seems doubtful or erroneous to the catalog compilers --- NoteFlag1 Notes in published catalog See the document by Kukarkin et al.(1982). There are several data fields that can contain asterisks. These signify that more complete information will be found in the remarks to the published catalog. The remarks are, unfortunately, not machine readable, but they do contain much supplemental information. There, one will find information covering situations like, e.g.: 1. The discoverer of the light variability is not the author of the paper cited in the variability reference, or is one of several authors of the paper cited. In these cases, discoverers' names are given in italics in original transcriptions of the remarks. 2. The most important additional information about a star, although the NSV compilers did not intend to present complete bibliographies for any catalogued stars. 3. Remarks for visual binaries (in parentheses following the number of a star in the corresponding catalog) giving visual magnitudes for the individual components A and B, angular separations, and position angles for faint components (or semimajor axis of a relative orbit and period of orbital motion). Data for other components are then given where applicable. (Combined magnitudes are generally reported in the machine-readable table.) --- RAh Hours RA, equinox 1950.0 The position is not listed when the variable is equivalent to a GCVS star (column VarName). h RAm Minutes RA, equinox 1950.0 min RAs Seconds RA, equinox 1950.0 s DE- Sign Dec, equinox 1950.0 --- DEd Degrees Dec, equinox 1950.0 deg DEm Minutes Dec, equinox 1950.0 arcmin DEs Seconds Dec, equinox 1950.0 arcsec u_DEs accuracy flags The actual accuracy of coordinates is indicated with the symbols: (:) means right ascensions accurate to one second of time and declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. --- VarType Type of variability type of variability. The system of variable star classification corresponds to the GCVS4 (see file "vartype.txt"). --- magMax Magnitude at maximum brightness Magnitudes are reported to hundredths if the observations are photoelectric, to tenths or whole magnitudes if they are not. If only an amplitude has been measured photoelectrically, then the maximum magnitude is generally given to tenths only and the minimum is reported to hundredths. mag u_magMax Uncertainty flag on magMax --- l_magMin "<" if magMin is a bright limit "(" if magMin is an amplitude; with "><" prefix, the amplitude in the table is a lower or upper limit. --- magMin Minimum magnitude or amplitude mag u_magMin a light amplitude is reported for the minimum and it is given in steps Uncertainty flag (:) on magMin --- f_magMin ")" if magMin is an amplitude --- magCode The photometric system for magnitudes The photometric system in which magMin and magMax are reported (see also Note on n_magMax, n_magMin). The main codes are P (photographic magnitudes) and V (visual, photovisual, or Johnson's V). --- Ref1 Reference to a study of the star see the document by Kukarkin et al.(1982) Usually a 6-digit number coding, as a rule, the reference to the announcement of the discovery of variability. The first two digits give the year (in the 20th century) when the announcement was published (blank for the 19th century). The next four digits give the number in the list of references contained in the published catalog, which is generally the first publication announcing the possible variability. The numbers are followed by a letter code in most cases (byte 57) with the following meanings: K: the cited paper contains a chart or photograph of the field with the suspected variable marked. D: the cited paper does not contain a chart, but the star is catalogued in one of the Durchmusterungen (DM) (BD,CD,CPD). --- Desig Designation in paper Ref1 The identification of the suspected variable in the paper referenced above. DM numbers are given without a prefix, the standard naming convention of "The Henry Draper Catalogue" being used (BD for zones +89 to -22; CD for -23 to -51; CP for -52 to -89). Some identifications are given by coordinate designations, a 6-digit number consisting of hours, minutes, and seconds (or tenths of a minute) of time and degrees of declination with sign included. An asterisk (*) signifies that a designation is given in the remarks to the published catalog. Stars are sometimes designated with numbers from the catalogs of Zinner (ZI, 1929) and Prager (PR, 1934, 1937) because the original discovery publications were not available to the NSV compilers. The catalogs of Zinner and Prager give detailed references to early observations of such stars. --- SpType Spectral type Temperature classes and subclasses only are given. Most luminosity classes are III to V, but if a star is a supergiant, more detailed classification information is given in the remarks to the published catalog. The following symbols are used: AF A-F AM Am AP Ap BE Be E emission spectrum EA e sub alpha EV variable emission in spectrum FG F-G KM K-M OF Of PD Pd T characteristics of T Tauri stars --- Ref2 Chart reference see the document by Kukarkin et al.(1982) The coding for the numbers is similar to that used in the variability references described above, except that there are no letter codes. These are references to papers containing identification charts if no charts are given in the papers cited for the variability references. --- VarName Designation in GCVS 1) The alternative name of the variable. All necessary information on the star is to be found under that alternative name, in the gcvs.dat file. 2) The star's name in the GCVS Vol. V (see the file v.zip, where the explanation of the designations is also given). In this case, the symbol "*" in column 89 means the presence of remarks in Vol. V. --- NoteFlag2 Notes in catalog GCVS Vol.V --- vartype.txt Description of variability types N.N. Samus, O.V. Durlevich Moscow Inst. F. Ochsenbein CDS 1999 Apr 21 The ADC thanks Drs. Samus and Durlevich for providing us with the up-to-date, machine-readable version of the GCVS and the Name Lists. This ReadMe is based on the one prepared by them and the four *.txt. in original documents: The computer-readable version of the Name-List files has been compiled by O.V. Durlevich, N.A.Gorynya, E.V.Kazarovets, and N.N. Samus, with the assistance of E.N.Pastukhova. We wish to thank O.Yu.Malkov for his kind consultations during the preparation of the first computer-readable version of Name-Lists. Thanks are due to S.V. Antipin for his assistance during GSC identifications and positional determinations. The crossid.dat was supported in part by the Russian Foundation for Basic Research (grant 95-02-05189) and by the Federal Program 'Astronomy' (grant 93-3-182). The authors gratefully acknowledge the financial support of the work on variable star catalogues by the International Astronomical Union until 1994. The final stage of the work on evs*.dat and sn*.dat was also supported by the European Southern Observatory (grant ESO C&EE A-02-047). The variable star studies were also sponsored through a grant of the Russian Federation programme "Astronomy". The authors are grateful to the American Association of Variable Star Observers who provided a grant for us in 1994. The printing of the book version was supported by the Russian Foundation for Basic Research. The Sternberg Institute part of the author team is grateful for the grant supplied through the program "Universities of Russia" in 1993. They wish to thank all astronomers who sent us their results prior to publication, gave us good advice, helped practically or with ideas. We would like to thank specially Drs. S.V. Antipin, V.P. Arkhipova, M. Bessell, Yu.N. Efremov, M.P. Galkina, Sh. Hughes, K.V. Kuimov, V.G. Kurt, T. Lloyd Evans, C. Lopez, R.I. Noskova, A.S. Sharov, Yu.A. Shokin, D.Yu. Tsvetkov, A.V. Zharov, A.V. Zharova. Authors' addresses: N.N. Samus [Moscow Inst. Astron.] O.V. Durlevich [Sternberg Astron. Inst., Moscow] <gcvs@sai.msu.su> UNKNOWN UNKNOWN This catalogue gathers the files previously numbered <II/139> (GCVS4, vols I-III), <II/172> (GCVS4, vol, IV), <II/205> (GCVS4, vol. V), <II/140> (New Suspected Variables), and <II/195> (Name-Lists). Catalogues <II/139> and <II/140> were first documented by Warren (1988, 1989); the documentation for the catalogues <II/172> and <II/205> was prepared by N.N. Samus and O.V. Durlevich (Moscow), with F. Ochsenbein (CDS). The first version of this Combined Catalogue (September 1997) was prepared by N. Roman (ADC) with the help of N.N. Samus and O.V. Durlevich (Moscow). The second version of this Combined Catalogue (August 1998), which incorporates the 73rd Name-List of Variable Stars and improved equatorial positions in Andromeda, Antlia and Apus, was prepared by N.N. Samus and O.V. Durlevich. Files were slightly reformatted at CDS (F. Ochsenbein) to have searchable epochs. The version 1.2 of the file "crossid.dat" was included on 22 May 1999. A further correction (QW Nor = NSV 7374 instead of NSV 7334) was applied on 16-Jun-1999 at CDS (message from N.N. Samus to F. Ochsenbein) II_214A.xml Sternberg Astronomical Institute Supernova Catalogue (1998July Version) 2218 II/218 Sternberg Supernova Catalogue Sternberg Astronomical Institute Supernova Catalogue (1998July Version) D Yu Tsvetkov N N Pavlyuk O S Bartunov SAISN group ??? ??? 1998 1998 II/159 : Asiago Supernova Catalogue 1988 (Barbon+, 1989) http://www.sai.msu.su/sn/ : the Sternberg Supernova Catalogue Home Page http://www.supernovae.org/isn.htm : International Supernovae Network http://www.astro.princeton.edu/~richmond/sn.list : Richmond's list of SNe Supernovae Surveys The catalogue presents the main data on 1362 extragalactic supernovae (SNe) discovered up to July 13, 1998 and on their parent galaxies. SNe are ordered by Right Ascension of their parent galaxies. Data for parent galaxies were compiled from the following catalogues: RC3 (de Vaucouleurs et al., 1991, Cat. <VII/155>); UGC (Nilson, 1973. Cat. <VII/26>); PGC (Paturel et al., 1989, Cat. <VII/119>); MCG (Vorontsov-Velyaminov et al., 1962-1968, Cat. <VII/62>, <VII/100>); ESO (Lauberts, 1982, Cat. <VII/34>); CfA (Huchra et al., 1994, see Cat <VII/193>), and from van den Bergh (1994, Cat. <J/ApJS/92/219>). Main source of morphological types, major diameters and axial ratios was the RC3; the data from other sources have been reduced to the system of RC3. Photographic magnitudes of galaxies were adopted from the UGC and the PGC together with individual data from the literature. The sources of recession velocities or cz values were the RC3, the CfA, the PGC and IAU Circulars. Position angles were taken from the RC3, UGC and the ESO catalogues, and inclination angles were mainly derived from data in RC3 according to Holmberg (1958MeLu2.136....1H). Some data for SNe and parent galaxies were adopted from GCVS (Samus et al., 1995, Cat. <II/205>)
The Catalog SN SN designation --- Gname Galaxy identification from NGC (N), IC (I), MCG (M), UGC (U) and ESO (E) catalogues. --- RAGh Galaxy Right Ascension (2000.0) h RAGm Galaxy Right Ascension (2000.0) min DEG- Galaxy Declination (2000.0) --- DEGd Galaxy Declination (2000.0) deg DEGm Galaxy Declination (2000.0) arcmin Gmag Photographic magnitude of Galaxy mag r_Gmag Source of magnitude 1 = from PGC catalogue, 2 = from the IAU Circular reporting SN discovery. 3 = "very uncertain magnitudes from different sources" (occurs for 1991P and 1991ao) --- Gpa Position angle measured from North to East deg Gi Inclination angle for disk-like systems (i = 0 for face-on systems) deg GVhel Heliocentric recession velocity km/s u_GVhel Uncertainty flag (:) on GVhel --- Gtype Morphological type --- GlogR Decimal log of axial ratio --- GlogD Decimal log of apparent isophotal major diameter [0.1arcmin] GTRC3 Numerical code of morphological type as in RC3 --- GLcRC3 Luminosity class as in RC3 --- EWoff E/W offset of SN in arcsec from the nucleus of the parent galaxy arcsec EW East or West direction --- NSoff N/S offset of SN from nucleus arcsec NS North or South direction --- mag Magnitude at maximum: Photographic or band mag l_mag Note about the magnitude ">" means "brighter than or equal to", "=" denotes the magnitude at maximum. --- n_mag Passband of photometry --- u_mag Uncertainty flag (:) on mag --- datMax Date of maximum light --- datDisc Date of discovery --- Type SN type --- RAh SN Right Ascension (2000.0) h RAm SN Right Ascension (2000.0) min RAs SN Right Ascension (2000.0) s DE- SN Declination (2000.0) --- DEd SN Declination (2000.0) deg DEm SN Declination (2000.0) arcmin DEs SN Declination (2000.0) arcsec Uncert "?" and "??" designate uncertain and very uncertain SN. --- Disc Code for SN search programme (Observatory) Observatory code where SN was discovered: AS Asiago Observatory BA Berkeley Automatic SN search BE Beijing Astronomical Observatory Supernova Survey (Weidong Li, Qiran Qiao, Yulei Qiu, Jingyao Hu); CA Cote d'Azur Observatory CR Cerro el Roble Observatory CT Cerro Tololo Observatory ER Experience de Recherche d'Objets Sombres (EROS) collaboration (O. Perdereau, J.C.Hamilton); EV Visual SN search of R.Evans GA Sternberg Astronomical Institute HB Supernovae discovered with help of HST HZ High-Z Supernova Search Team (R.P. Kirshner, P. Garnavich, P. Challis et al.); IT Italian Professionals and Amateurs; (S. Pesci, M. Villi, A. Gabrielcic et al. ) JP Other Japanese Professionals and Amateurs (Aoki, K. Okazaki et al.); KO Konkoly Observatory KU Supernovae discovered by R. Kushida, Yatsugatake South Base Observatory, Japan; MD University of Texas McDonald Observatory Supernova Search Team (M.T. Adams, T. Montemayor, D.A. Howell, J.C. Wheeler, M.H. Ward, and W. Wren) MN SNe discovered by R.H.McNaught MS Mount Stromlo Abell Cluster Supernova Search Team (L. Germany, D. Reiss, C. Stubbs, B. Schmidt, S. Chan); P1 Palomar Observatory SN search 1958-1974 P2 Palomar Observatory SN search 1937-1940 P3 SNe discovered on POSS plates P4 SNe discovered on plates of second POSS PE Perth observatory supernova search program (A. Williams and R. Martin); SC The Supernova Cosmology Project (S. Perlmutter et al.); TE Supernovae discovered by M. Schwartz (Tenagra Observatory, Oregon, USA); WJ Supernovae discovered by W. Johnson, CA; ZM Zimmerwald Observatory --- Text Discoverer and comments; the asterisk (*) indicates a note in file "notes.dat" --- Notes to individual supernovae. SN SN designation --- Text Text of note --- Francois Ochsenbein CDS 1998 Oct 26 N.Pavlyuk <pavlyuk@sai.msu.su> Michael Schwartz (Tenagra Observatory, Oregon, USA) II_218.xml New Catalogue of Suspected Variable Stars. Supplement - Version 1.0 2219 II/219 New Catalogue of Suspected Variable Stars Supplement New Catalogue of Suspected Variable Stars. Supplement - Version 1.0 E V Kazarovets O V Durlevich N N Samus Institute of Astronomy of Russian Academy of Sciences and Sternberg Astronomical Institute ??? ??? 1988 1998IBVS.4655....1K II/214 : The combined GCVS4.1 (Kholopov+, 1998) ftp://ftp.sai.msu.su, /pub/groups/cluster/gcvs/gcvs/nsvsup/ : (anonymous) http://www.sai.msu.su/groups/cluster/gcvs/gcvs/ : GCVS pagesKholopov, P. N., Samus, N. N., Frolov, M. S., Goranskij, V. P., Gorynya, N. A., Karitskaya, E. A., Kazarovets, E. V., Kireeva, N. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Rastorguev, A. S., and Shugarov, S. Yu. 1985-1988, "General Catalogue of Variable Stars", 4th Edition, Volumes I-III, (Moscow: Nauka Publishing House). Kukarkin, B. V., Kholopov, P. N., Artiukhina, N. M., Fedorovich, V. P., Frolov, M. S., Goranskij, V. P., Gorynya, N. A., Karitskaya, E. A., Kireeva, N. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Ponomareva, G. A., Samus, N. N., and Shugarov, S. Yu. 1982, "New Catalogue of Suspected Variable Stars", (Moscow: Nauka Publishing House). Kholopov, P. N., Samus, N. N., Durlevich, O. V., Kazarovets, E. V., Kireeva, N. N., Tsvetkova, T. M. 1990, "General Catalogue of Variable Stars", 4th Edition, Vol. IV, (Moscow: Nauka Publishing House). Kholopov, P. N., Samus, N. N., Frolov, M. S., Goranskij, V. P., Kazarovets, E. V., Kireeva, N. N., Perova, N. B. 1985-1995, "Name-lists of variable stars Nos. 67-72". Artyukhina, N. M., Durlevich, O. V., Frolov, M. S., Goranskij, V. P., Gorynya, N. A., Karitskaya, E. A., Kazarovets, E. V., Kholopov, P. N., Kireeva, N. N., Kurochkin, N. E., Lipunova, N. A., Medvedeva, G. I., Pastukhova, E. N., Samus, N. N., Tsvetkova, T. M. 1995, "General Catalogue of Variable Stars", 4th Edition, Vol. V: Extragalactic Variable Stars (Moscow: "Kosmosinform"). Stars, variable This catalog is a compilation of 11206 stars suspected of variability and not finally designated as variables prior to 1997. It is the supplementary part to the "New Catalogue of Suspected Variable Stars" published in 1982 (Kukarkin et al., file "nsv.dat" included here). Data contained in the present catalog include positions, magnitudes, variability types, references to the literature, spectra and cross-identifications. The computer version of the NSV Supplement contains principally the same data as the printed catalog, the data tables with the textual material (bibliography, remarks) are included.
The NSV Supplement Catalog NSV NSV number --- RemFlag indicates a remark in file remark.dat There are several data fields that can contain asterisks. These signify that more complete information will be found in the remarks to the published catalog. The remarks are machine readable, they do contain much supplemental information. There, one will find information covering situations like, e.g.: 1. The discoverer of the light variability is not the author of the paper cited in the variability reference, or is one of several authors of the paper cited. In these cases, discoverers' names are given in original transcriptions of the remarks. 2. The most important additional information about a star, although the NSV Supplement compilers did not intend to present complete bibliographies for any catalogued stars. 3. Remarks for visual binaries giving visual magnitudes for the individual components A and B, angular separations, and position angles for faint components (or semimajor axis of a relative orbit and period of orbital motion). Then, data for other components are given where applicable. (Combined magnitudes are generally reported in the machine-readable table.) --- RAh Hours RA, equinox 1950.0 h RAm Minutes RA, equinox 1950.0 min RAs Seconds RA, equinox 1950.0 s DE- Sign Dec, equinox 1950.0 --- DEd Degrees Dec, equinox 1950.0 deg DEm Minutes Dec, equinox 1950.0 arcmin DEs Seconds Dec, equinox 1950.0 arcsec u_DEs accuracy flags The actual accuracy of coordinates is indicated with the symbols: (:) means right ascensions accurate to one second of time and declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. --- RA2000h Hours RA, equinox 2000.0 h RA2000m Minutes RA, equinox 2000.0 min RA2000s Seconds RA, equinox 2000.0 s DE2000- Sign Dec, equinox 2000.0 --- DE2000d Degrees Dec, equinox 2000.0 deg DE2000m Minutes Dec, equinox 2000.0 arcmin DE2000s Seconds Dec, equinox 2000.0 arcsec VarType Type of variability Type of variability. The system of variable star classification corresponds to the GCVS4, with six additions (ZZO, AM, R, BE, LBV, BLBOO) introduced in the Name-Lists 67-72 and in the GCVS vol.V. Brief descriptions only are given here: ACV, ACVO Alpha2 Canum Venaticorum ACYG Alpha Cygni BCEP, BCEPS Beta Cephei BE Be BL BL Lacertae BY BY Draconis CEP Cepheid CST constant CW W Virginis DCEP Delta Cephei DSCT, DSCTC Delta Scuti E eclipsing EA Algol (Beta Persei) EB Beta Lyrae EW W Ursae Majoris ELL ellipsoidal FKCOM FK Comae Berenices FU FU Orionis GAL galaxy GCAS Gamma Cassiopejae I irregular IA, INA white irregular IB, INB red irregular IN irregular in a nebula IT, INT irregular of the T Tauri type IS, ISA rapid irregular L slow LB slow red LBV long-period pulsating B star M Mira (Omicron Ceti) type N Nova NL nova-like NR recurrent Nova QSO quasistellar object RR RR Lyrae RS RS Canum Venaticorum RV RV Tauri S rapid SN supernova SR, SRA, SRB, SRD semiregular SXARI SX Arietis SXPHE SX Phoenicis UG U Geminorum UGSS SS Cygni UV UV Ceti VAR variable WR Wolf-Rayet star XM X-ray system with a strong magnetic field XNA X-ray nova-like ZAND Z Camelopardalis ZZA, ZZO ZZ Ceti --- l_magMax "<" if magMax is a bright limit, ">" if magMax is a faint limit, --- magMax Magnitude at maximum brightness The star's magnitude in minimum and maximum brightness. Instead of the magnitude in minimum, the star's amplitude of variation may be indicated (in brackets). Magnitudes are reported to hundredths if the observations are photoelectric or CCD, to tenths or whole magnitudes if they are not. If only an amplitude has been measured photoelectrically, then the maximum magnitude is generally given to tenths only and the minimum is reported to hundredths. mag u_magMax Uncertainty flag on magMax --- l_magMin "(" if magMin is an amplitude; with "><" prefix, the amplitude in the table is a lower or upper limit --- magMin Minimum magnitude or amplitude mag n_magMin The photometric system for amplitudes The photometric system in which magMin and magMax are reported. The main codes are V (visual, photovisual, or Johnson's V), B (Johnson's B) and P (photographic magnitudes). The designations u, v, b, y refer to the Stroemgren system. The symbols Ic, Rc mean magnitudes in Cousins' I, R system; Hp, T - in Hipparcos and Tycho mission systems; J, H, K, L, M - infrared magnitudes. --- f_magMin ")" if magMin is an amplitude --- u_magMin Uncertainty flag (:) on magMin or amplitude --- magCode The photometric system for magnitudes and amplitudes --- r_NSV Reference to a study of the star (see file refs.dat) The four digits give the number in the list of references contained in the catalog, which is generally the first publication announcing the possible variability. --- Ref2 Chart reference (see file refs.dat) The coding for the numbers is similar to that used in the variability references described above, except that there are also letter codes. These are references to papers containing identification chart or photograph of the field with the suspected variable marked. If the cited paper does not contain a chart, but the star is catalogued in one of the Durchmusterungen (BD,CD,CPD) or in the Hubble Space Telescop Guide Star Catalog (GSC), then corresponding letter codes DM or GSC are given. --- SpType1 Spectral type Spectral types, subtypes and luminosity classes are given. More detailed classification information is given in the remarks to the catalog. Also the following symbols are used: AF A-F cont continuum e emission spectrum ea e sub alpha FG F-G KM K-M * see Sp type in remarks --- SpType2 Spectral type from HD catalog in brackets --- VarName Designation in GCVS The alternative name of the variable. All necessary information on the star is to be found under that alternative name in Cat. <II/214> (file gcvs.dat) --- Identifications NSV NSV number --- --- Equality sign --- ID Identifications all identifications needed to find the star in the papers with the first (or independent) announcement of the discovery of its variability. References to these papers (see file refs.dat) are given in square brackets after the corresponding identification. The name of the discoverer accompanies the reference only in the case of its being different from the name of the author(s) of the paper referred to. Designations of components of double or multiple system: A, B, C, ..., A1, A2, ..., p - preceding, f - following, s - southern, n - northern. The transliterations of greek letters are used: alpha, beta, gamma,..., omega, etc., kappa 2, omicr 1. Different identifications of the same star with catalogs and lists are separated with equality sings (=). Symbol (?) marks the doubtful identification. The following catalogs abbreviations are used (abbreviated names for some of them are presented): Bayer - Greek and Roman letters in the Bayer Atlas, Flamsteed - Baily, F. 1835, "Association of J.Flamsteed, British Catalogue of Stars". BS (HR) - Hoffleit, D. (with the collaboration of Jaschek, C.) 1982, "The Bright Stars Catalogue" (New Haven: Yale University Observatory) (HR numbers are adopted from Pickering, E. C., 1908, "Harvard Revised Photometry", Ann. Astron. Obs. Harvard College 50). (See Cat. <V/50>) HD - Cannon, A. J. and Pickering, E. C. 1918-1924, "The Henry Draper Catalogue", Ann. Astron. Obs. Harvard College 91-99. (See Cat. <III/135>) BD - Argelander, F. 1859-62, "Bonner Sternverzeichniss. Erste bis dritte Sektion", Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rhein. Friedrich-Wilhelms-Universitaet zu Bonn, Bande 3-5. Revision of Argelander's first edition: Schoenfeld, E. 1886, "Bonner Sternverzeichniss", Vierte Sektion, Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rheinischen Friedrich-Wilhelms-Universitaet zu Bonn 8, Part IV (Bonn: Adolph Marcus); Kuestner, F. 1903, "Bonner Durchmusterung des Noerdlichen Himmels, zweite berichtigte Auflage", Bonn Universitaets-Sternwarte. (See Cats <I/122> and <I/119>) CoD - Thome, J. M. 1892-1932, "Cordoba Durchmusterung, Resultados del Observatorio Nacional Argentino" 16 (1892, Part I: -22 to -32 Degrees), 17 (1894, Part II: -32 to -42 Degrees), 18 (1900, Part III: -42 to -52 Degrees), 21 (Part I) (1914, Part IV, -52 to -62 Degrees), 21 (Part II) (1932, Part V: -61 to -90 Degrees). (See Cat. <I/114>) CPD - Gill, D. and Kapteyn, J. C. 1895-1900, "Cape Photographic Durchmusterung", Ann. Cape Obs. 3 (1895, Part I: zones -18 to -37); 4 (1897, Part II: zones -38 to -52); 5 (1900, Part III: zones -53 to -89). (See Cat. <I/108>) GSC - Lasker, B. M., et al. 1990, "The Guide Star Catalog. I. Astronomical Foundations and Image Processing", A. J. 99, 2019; The Space Telescope Science Institute 1992, "The Guide Star Catalog Version 1.1 (An all-sky astrometric and photometric catalog to support the operation of the Hubble Space Telescope)" on two CD-ROMs. (See Cat. <I/220>) HIP - European Space Agency 1997, "The Hipparcos and Tycho Catalogues", SP-1200, Vols. 1-17. (See Cat. <I/239>) SAO - Smithsonian Astrophysical Observatory Staff 1966, "Star Catalog. Positions and Proper Motions of 258,997 Stars for the Epoch and Equinox of 1950.0", Publ. of the Smithsonian Institution of Washington, D.C., No. 4652. (See Cat. <I/131>) ADS - Aitken, R. G. 1932, "New General Catalogue of Double Stars within 120 Degrees of the North Pole", Carnegie Institution of Washington, Publ. no. 417 (Washington, D.C.: Carnegie Institution of Washington). IDS - Jefers, H. M., Van den Bos, W. H., Greeby, F. M. 1963, "Index Catalogue of Visual Double Stars", Publ. Lick Obs. 21. BDS - Burnham, S. W. 1906, "A General Catalogue of Double Stars within 120 Degrees of the North Pole", Carnegie Institution of Washington, Publ. No. 5 (Washington, D.C.: Carnegie Institution of Washington). CCDM - Dommanget, J., Nys, O. 1994, "The Catalogue of Components of Double and Multiple Stars", Comm. Obs. R. de Belg., Serie A No.115 (catalog CDS <I/211>). IRC - Neugebauer, G. and Leighton, R. B. 1969, "Two-Micron Sky Survey, A Preliminary Catalog", NASA SP-3047 (Washington, D.C.: National Aeronautics and Space Adminstration). (See Cat. <II/2>) AFGL/RAFGL - Walker, R. G., Price, S. D. 1975, "Air Force Cambridge Research Laboratory Infrared Sky Survey", U.S. Air Force Report No. AFCRL-TR-0373; Price, S. D., Walker, R. G. 1976 "The AFGL Four Color Infrared Sky Survey", AFGL-TR-0208, and 1977 "The AFGL Four Color Infrared Sky Survey Supplement", AFGL-TR-0160. IRAS - The Joint IRAS Science Working Group 1988, "Infrared Astronomical Satellite (IRAS) catalogs and atlases" 2-6, NASA RP-1190 (Washington, D.C.: National Aeronautics and Space Adminstration). (See Cat. <II/125>) MWC - Merrill, P. W., Sunford, R. F., Burwell, C. G. 1933-1949, "Mount Wilson Catalogue of stars of classes B and A whose spectra have bright hydrogen lines", P.A.S.P. 45, 306; P.A.S.P 54, 107; Ap. J. 78, 87; Ap. J. 98, 153; Ap. J. 110, 387. AS - Merrill, P. W., Burwell, C. G. 1950, "Additional stars whose spectra have a bright H Alpha line", Ap. J. 112, 72. LkHa - Herbig, G. H., et al. 1954-1974, Lists of emission-line stars. MHa - Mount Wilson H Alpha-emission line stars, see references for MWC and AS. He-3 - Henize, K. G. 1976, "Observations of Southern Emission-Line Stars", Ap. J. Suppl. 30, 491. HRC/HBC - Herbig, G. H., Robbin Bell, K. 1988, "Third Catalog of Emission-Line Stars of the Orion Population", Lick Obs. Bull No.1111. Wray - Wray, J. D. 1966, "A study of H Alpha-emission objects in the Southern Milky Way", Table XV-XIX, Univ. Microfilm Inc., Ann Arbor, Michigan. LS - Hardorp, J., et al. 1959-1971, "Luminous Stars in the Northern Milky Way" I-VI, Hamburger Sternwarte - Warner and Swasey Obs., Hamburg-Bergedorf. (See Cat. <III/76>) LSS - Stephenson, C. B., Sanduleak, N. 1971, "Luminous Stars in the Southern Milky Way", Publ. Warner and Swasey Obs. 1, No.1. (See Cat. <III/43>) CCS - Stephenson, C. B. 1973, "A General Catalogue of Cool Carbon Stars", Publ. Warner and Swasey Obs. 1, No.4. (See Cat. <III/156>) Hen - Unpublished list of C-stars by K.G.Henize (given in CCS), CSS - Stephenson, C. B. 1976, "A General Catalogue of S Stars", Publ. Warner and Swasey Obs. 2, No.2. (See Cat. <III/60>) WR - Van der Hucht, K. A., et al. 1981, "The Sixth Catalogue of Galactic Wolf-Rayer Stars", Space Sci. Rev. 28, 227. PG - Green, R. F., et al. 1986, "Cataclysmic Variable Candidates from the Palomar Green Survey", Ap. J. Suppl. 61, 305. (See Cat. <II/207>) WD - McCook, G. P., Sion, E. M. 1987, "A Catalogue of Spectroscopically Identified White Dwarfs", Ap. J. Suppl. 65, 603. (See Cat. <III/129>) G - Giclas, H. L., et al. 1971-1979, "Lowell Proper Motion Survey" (red dwarfs), Lowell Obs. Bull., Flagstaff, Arizona. GD - Giclas, H. L., et al. 1980, "Lowell Proper Motion Survey" (white dwarfs), Lowell Obs. Bull. 8, 157. Eg/Gr - Eggen, O. J., Greenstein, J. L. 1965-1977, "Spectra, Colors, Luminosities and Motions of the White Dwarfs", Ap. J. 141, 83; Ap. J. 142, 925; Ap. J. 150, 927; Ap. J. 158, 281; Ap. J. 162, L55; Ap. J. 189, L131; Ap. J. 196, L117; Ap. J. 207, L119; Ap. J. 218, L21. Gliese - Gliese, W. 1969, "Catalogue of Nearby Stars", Veroeff. Astron. Rechen-Inst. Heidelberg Nr.22; Gliese, W., Jahreiss, H. 1979, "Nearby star data published 1969-1978", Astron. Astrophys. Suppl. 38, 423. (See Cat. <V/70>) He-2 - Henize, K. J. 1964, An extended list of southern planetary nebulae; see PK Nomenclature. PK - Perek, L., Kohoutek, L. 1967, "Catalogue of Galactic Planetary Nebulae", Academia Publishing House of the Czechoslovak Academy of Sciences. NGC - Dreyer, J. L. E. 1888, "New General Catalogue of Nebulae and Clusters of Stars", Mem. Roy. Astron. Soc. 49, Part I (reprinted 1962, London: Royal Astronomical Society); Sulentic, J. W. and Tifft, W. G. 1973, "The Revised New General Catalogue of Nonstellar Astronomical Objects" (Tucson: The University of Arizona Press). (See Cat. <VII/118>) LHS - Luyten, W. J. 1976, "A Catalog of Stars with Proper Motion exceeding 0".5 annually", Publ. of Univ. of Minnesota, Minneapolis, Minnesota; Luyten, W. J., Albers, H. 1979, "An Atlas of Identification Chart for LHS Stars", Publ. of Univ. of Minnesota, Minneapolis, Minnesota. (See Cat. <I/87>) LTT - Luyten, W. J. 1957, "Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motion exceeding 0".2 annually"; Luyten, W. J. 1961, "Catalogue of 7127 Stars in the Northern Hemisphere with Proper Motion exceeding 0".2 annually", The Lund Press, Minneapolis, Minnesota. LFT - Luyten, W. J. 1955, "A Catalog of 1849 Stars with Proper Motion exceeding 0.5" annually", The Lund Press, Minneapolis, Minnesota. L - Luyten, W. J. 1941, "Proper Motion Survey with the fourty-eight inch Schmidt Telescope", XXI, XXV, XXIX, Publ. of Univ. of Minnesota. LP - Luyten, W. J. 1963-1981, "Proper Motion Survey with the 48 inch Schmidt Telescope", Publ. of Univ. of Minnesota, Minneapolis, fasc. 1-57. LDS - Luyten, W. J. 1943, "Catalogue of 832 Double Stars with Common Proper Motion in the Southern Hemisphere", Publ. Astron. Obs. Univ. Minnesota 3, No. 3, 33. BPM - Luyten, W. J. 1963, "Bruce Proper Motion Survey. The general catalogue. Vol. I, II", Publ. of Univ. of Minnesota, Minneapolis, Minnesota. Ross - Ross, F. E. 1925-1939, "New Proper Motion Stars", eleven successive lists, A. J. Vol. 36 to 48. Vys - Vyssotsky, A. N., et al. 1943-1958, "Dwarf M Stars Found Spectrophotometrically", A. J. 61, 201; A. J. 63, 211; Ap. J. 97, 381; Ap. J. 104, 234; Ap. J. 116, 117. Wolf - Wolf, M. 1919, "Katalog von 1053 starken bewegten Fixsternen", Veroeff. Sternwarte zu Heidelberg 7, No. 10, 195; and numerous lists in Astron. Nachr. 209 to 236, 1919 to 1929. OH - OH sources designated by their galactic co-ordinates. HII - Hertzsprung, E. 1947, "Catalogue de 3259 Etoiles dans les Pleiades", Ann. Sterrewacht Leiden 19, part 1A. Par - Parenago, P. P. 1954, "A List of Star in the Region of the Orion Nebula", Trudy Sternberg Astron. Inst. Vol. 25. HV - Preliminary designations of variables discovered at Harvard Observatory. S - Preliminary designations of variables discovered at Sonneberg Observatory. SVS - Soviet variable stars (preliminary designations of Soviet-discovered variables). VV - Preliminary designations of variables discovered at Vatican. VES - Lists of the Vatican H Alpha-emission line stars. --- Remarks NSV NSV number --- Text Text of remark See Note on RemFlag (nsvs.dat) and Note on ID (ident.dat). --- References Ref Reference number --- Text Text of reference We attempted to give Latin transliterations of Russan-language names of astronomical periodicals and books. We did not try to unify the Latin spelling of names with Cyrillic (or other) original forms, but simply tried to reproduce the Latin transcriptions in the publications referred to. When several lines are needed, the reference number is repeated. The "bibcode", if known, is added at the beginning of the text. --- *New Suspected Variables (Kukarkin et al. 1982) NSV NSV number --- m_NSV NSV letter suffix The letter "A" is present for one star, NSV 10360A, which is a completely different object from NSV 10360. --- u_NSV Dubitancy flag if a star's variability seems doubtful or erroneous to the catalog compilers --- NoteFlag1 Notes in published catalog see the document by Kukarkin et al.(1982) There are several data fields that can contain asterisks. These signify that more complete information will be found in the remarks to the published catalog. The remarks are, unfortunately, not machine readable, but they do contain much supplemental information. There, one will find information covering situations like, e.g.: 1. The discoverer of the light variability is not the author of the paper cited in the variability reference, or is one of several authors of the paper cited. In these cases, discoverers' names are given in original transcriptions of the remarks. 2. The most important additional information about a star, although the NSV compilers did not intend to present complete bibliographies for any catalogued stars. 3. Remarks for visual binaries (in parentheses following the number of a star in the corresponding catalog) giving visual magnitudes for the individual components A and B, angular separations, and position angles for faint components (or semimajor axis of a relative orbit and period of orbital motion). Data for other components are then given where applicable. (Combined magnitudes are generally reported in the machine-readable table.) --- RAh Hours RA, equinox 1950.0 The position is also listed when the variable is equivalent to a GCVS star (column VarName). h RAm Minutes RA, equinox 1950.0 min RAs Seconds RA, equinox 1950.0 s DE- Sign Dec, equinox 1950.0 --- DEd Degrees Dec, equinox 1950.0 deg DEm Minutes Dec, equinox 1950.0 arcmin DEs Seconds Dec, equinox 1950.0 arcsec u_DEs accuracy flags The actual accuracy of coordinates is indicated with the symbols: (:) means right ascensions accurate to one second of time and declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. --- VarType Type of variability type of variability (see file ...\III\vartype.txt). The system of variable star classification corresponds to the GCVS4, with six additions (ZZO, AM, R, BE, LBV, BLBOO) introduced in the Name-Lists 67- 72 and in the GCVS vol.V. (see "Note on VarType" section above) --- magMax Magnitude at maximum brightness Magnitudes are reported to hundredths if the observations are photoelectric, to tenths or whole magnitudes if they are not. If only an amplitude has been measured photoelectrically, then the maximum magnitude is generally given to tenths only and the minimum is reported to hundredths. mag u_magMax Uncertainty flag on magMax --- l_magMin "<" if magMin is a bright limit "(" if magMin is an amplitude; with "><" prefix, the amplitude in the table is a lower or upper limit. --- magMin Minimum magnitude or amplitude mag u_magMin a light amplitude is reported for the minimum and it is given in steps Uncertainty flag (:) on magMin --- f_magMin ")" if magMin is an amplitude --- magCode The photometric system for magnitudes the photometric system in which magMin and magMax are reported (see also Note on n_magMax, n_magMin). The main codes are P (photographic magnitudes) and V (visual, photovisual, or Johnson's V). See also the documents by Kholopov et al. (1985-1988) or Warren (1988). --- Ref1 Reference to a study of the star see the document by Kukarkin et al.(1982) Usually a 6-digit number coding, as a rule, the reference to the announcement of the discovery of variability. The first two digits give the year (in the 20th century) when the announcement was published (blank for the 19th century). The next four digits give the number in the list of references contained in the published catalog, which is generally the first publication announcing the possible variability. The numbers are followed by a letter code in most cases (byte 75) with the following meanings: K: the cited paper contains a chart or photograph of the field with the suspected variable marked. D: the cited paper does not contain a chart, but the star is catalogued in one of the Durchmusterungen (DM) (BD,CD,CPD). --- Desig Designation in paper Ref1 The identification of the suspected variable in the paper referenced above. DM numbers are given without a prefix, the standard naming convention of "The Henry Draper Catalogue" being used (BD for zones +89 to -22; CD for -23 to -51; CP for -52 to -89). Some identifications are given by coordinate designations, a 6-digit number consisting of hours, minutes, and seconds (or tenths of a minute) of time and degrees of declination with sign included. An asterisk (*) signifies that a designation is given in the remarks to the published catalog. Stars are sometimes designated with numbers from the catalogs of Zinner (ZI, 1929) and Prager (PR, 1934, 1937) because the original discovery publications were not available to the NSV compilers. The catalogs of Zinner and Prager give detailed references to early observations of such stars. --- SpType Spectral type Spectral types and subtypes only are given. Most luminosity classes are III to V, but if a star is a supergiant, more detailed classification information is given in the remarks to the published catalog. The following symbols are used: AF A-F AM Am AP Ap BE Be E emission spectrum EA e sub alpha EV variable emission in spectrum FG F-G KM K-M OF Of PD Pd T characteristics of T Tauri stars --- Ref2 Chart reference see the document by Kukarkin et al.(1982) The coding for the numbers is similar to that used in the variability references described above, except that there are no letter codes. These are references to papers containing identification charts if no charts are given in the papers cited for the variability references. --- VarName Designation in GCVS 1) The alternative name of the variable. All necessary information on the star is to be found under that alternative name, in the iii.zip and nl.zip files. 2) The star's name in the GCVS Vol. V (see the file v.zip, where the explanation of the designations is also given). In this case, the symbol "*" in column 89 means the presence of remarks in Vol. V. --- NoteFlag2 Notes in catalog GCVS Vol.V --- E.V. Kazarovets, O.V. Durlevich Moscow & Sternberg 1999 May 10 UNKNOWN UNKNOWN * 16-Jun-1999: in file nsv.dat, the star NSV 7334 = HV 10762 which was erroneously cross-identified with QW Nor, was corrected at CDS (the original data of the 1982 version of the NSV catalogue were inserted for this star) QW Nor is identical to NSV 7374. II_219.xml Polarization of Be stars 2220 II/220 Polarization of Be stars Polarization of Be stars D McDavid Publ. Astron. Soc. Pacific 98 572 1986 1986PASP...98..572M Polarization of Be stars D McDavid Publ. Astron. Soc. Pacific 102 773 1990 1990PASP..102..773M Polarization of Be stars D McDavid Publ. Astron. Soc. Pacific 106 949 1994 1994PASP..106..949M Polarization of Be stars D McDavid Publ. Astron. Soc. Pacific 111 494 1999 1999PASP..111..494M Stars, Be Stars, variable Polarization The catalogue contains observations of the linear polarization in the UBVRI photometric system of 8 Northern Be stars; the observations are part of a long-term monitoring program begun in 1984.
Standard and Program Be stars ps Program or Standard star --- Name Star name --- HD HD (Cat. <III/135>) catalog number --- HR BS (Cat. <V/50>) catalog number --- Vmag Visual magnitude (BSC4, See Cat. <V/50>) mag RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Sp Spectral type number=1 According to Slettebak, A. 1982ApJS...50...55S (for program stars only) --- vsini projected rotational velocity number=1 According to Slettebak, A. 1982ApJS...50...55S (for program stars only) km/s Polarization of 2H Cam (standard star) Polarization of {omicron} Sco (standard star) Polarization of {gamma} Cas Polarization of {phi} Per Polarization of 48 Per Polarization of {zeta} Tau Polarization of 48 Lib Polarization of {chi} Oph Polarization of {pi} Aqr Polarization of {omicron} And Year Year of observation yr Filter Filter system passband number=1 the filters (effective wavelength and passbands) are: ------------- EffL FWHM ------------- U 3650 700 B 4400 1000 V 5500 900 R 6400 1500 I 7900 1500 ------------- --- nobs Number of observations --- q Mean normalized Stokes parameter q % e_q rms uncertainty on q % u Mean normalized Stokes parameter u % e_u rms uncertainty on u % p Mean degree of polarization % e_p rms uncertainty on p % theta Mean equatorial position angle deg e_theta rms uncertainty on theta deg dpi Instrumental precision of q, u, or p % dthetai Instrumental precision of theta deg D. McDavid Limber Observatory, Texas 1999 Feb 19 Author's Address: McDavid D. mcdavid@limber.org Limber Observatory, Timber Creek Road, P.O. Box 63599, Pipe Creek,Texas 78063 II_220.xml First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg 2223 II/223 First Byurakan Survey First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G V Abramyan V A Lipovetskii D A Stepanyan Astrophysics 32 14 1990 1990Ap.....32...14A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg H V Abrahamian V A Lipovetsky A M Mikaelyan J A Stepanian Astrophysics 33 418 1990 1990Ap.....33..418A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg H V Abrahamian K S Gigojan Astrophysics 33 493 1990 1990Ap.....33..493A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G V Abramyan V A Lipovetskii A M Mikaelyan J A Stepanian Astrophysics 34 7 1991 1991Ap.....34....7A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G B Abramyan A M Mikaelyan Astrophysics 36 62 1993 1993Ap.....36...62A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G B Abramyan A M Mikaelyan Astrophysics 36 306 1993 1993Ap.....36..306A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G B Abramyan A M Mikaelyan Astrophysics 37 27 1994 1994.....37...27A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G B Abramyan A M Mikaelyan Astrophysics 37 117 1994 1994Ap.....37..117A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G B Abramyan A M Mikaelyan Astrophysics 37 224 1994 1994Ap.....37..224A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G V Abramyan A M Mikaelyan Astrophysics 38 108 1995 1995Ap.....38..108A First Byurakan Spectral Sky Survey - Blue Stellar Objects - I. Region Dec = +39Deg G B Abramyan A M Mikaelyan Astrophysics 39 315 1996 1996.....39...315A VII/172 : First Byurakan Survey (FBS) (Markarian+, 1989) II/207 : Palomar-Green catalog UV-excess stellar objects (Green+ 1986) The references include the two paginations in the Russian Astrofizika and in the English translation Astrophysics for the papers published before 1994; they also indicate the limits in the Seq number of the sources in each publication. Abrahamian H.V., Lipovetsky V.A., Stepanian J.A. 1990Ap.....32...14A =1990Afz....32...29A ( 1- 100) Abrahamian H.V., Lipovetsky V.A., Mickaelian A.M., Stepanian J.A. 1990Ap.....33..418A =1990Afz....33..213A ( 101- 203) Abrahamian H.V., Lipovetsky V.A., Mickaelian A.M., Stepanian J.A. 1990Ap.....33..493A =1990Afz....33..317A ( 204- 323) Abrahamian H.V., Lipovetsky V.A., Mickaelian A.M., Stepanian J.A. 1991Ap.....34....7A =1991Afz....34...13A ( 324- 429) Abrahamian H.V., Mickaelian A.M. 1993Ap.....36...62A =1993Afz....36..109A ( 430- 540) Abrahamian H.V., Mickaelian A.M. 1993Ap.....36..306A =1993Afz....36..517A ( 541- 638) Abrahamian H.V., Mickaelian A.M. 1994Ap.....37...27A =1994Afz....37...43A ( 639- 757) Abrahamian H.V., Mickaelian A.M. 1994Ap.....37..117A =1994Afz....37..197A ( 758- 855) Abrahamian H.V., Mickaelian A.M. 1994Ap.....37..224A ( 856- 939) Abrahamian H.V., Mickaelian A.M. 1995Ap.....38..108A ( 940-1039) Abrahamian H.V., Mickaelian A.M. 1996Ap.....39..315A (1040-1103) Blue objects Galaxies, UV-excess The First Byurakan Survey (FBS), also known as the Markarian survey, covers about 17000 sq. deg. It has been used by Markarian and his collaborators to search for UV excess galaxies (see Cat. <VII/172>) and by Abrahamian and his collaborators to search for UV excess or emission line starlike objets. The identification, classification, and investigation of all blue stellar objects in the Survey constitutes the second part of the First Byurakan Survey and is a natural continuation of it. For this second program, at the present time, 4109 sq. deg. have been searched (33 < {delta} < 45 deg and {delta} > 61 deg, excluding the galactic plane) and a catalogue of 1103 blue stellar objects has been built. It has been published in a series of eleven papers referenced in the "References" section below. More details can be found in Mickaelian et al. 1999, Astrofizika 42,5: 'On the nature of the FBS blue stellar objects and the completeness of the Bright Quasar Survey'. Some accurate optical positions were measured by M. Veron, replacing the original FBS position.
The second part of the First Byurakan Survey Seq Sequential number (FBS B NNNN) --- FBS FBS named based on B1950 position --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec Bmag Photographic magnitude mag aType abbreviation for QSO, Galaxy or Star --- Type Type of the object this Type is made of two parameters: 1. The first parameter (related to B-V index) describes the ratio of the intensities of the red and blue regions of the spectrum: 'B' means that the blue part is stronger than the red part 'N' means that the intensities of the two parts are equal 2. The second parameter (related to U-B index) characterizes the intensity of the ultraviolet region of the spectrum: '1' means that the blue-violet part is approximately 1.5 times longer than the red-yellow part '3' means that the blue-violet part is approximately as long as the red-yellow part '2' describes the intermediate situation. In addition, the existence of emission details is noted by 'e' or 'e:', and absorption details by 'a' or 'a:' --- SpType Spectral type for stars --- survey Existence in other survey the other surveys are PG = Palomar Green survey (see Cat. <II/207>) CBS = Case Blue Stars (Pesch and Sanduleak, 1983-95) CSO = Case Stellar Objects (Pesch and Sanduleak, 1983-95) KUV = Kiso UV excess objects (Nogushi et al., 1980AnTok..18...55N) --- Mag2 Magnitude from survey mag z Redshift, when known --- Name Other name of the source --- Mira Veron OHP Francois Ochsenbein CDS 1999 Feb 11 UNKNOWN UNKNOWN The catalogue was typed in by Mira Veron <mira@obs-hp.fr> (Observatoire de Haute-Provence, France) II_223.xml The Asiago Supernova Catalogue - 10 years after 2227 II/227 The Asiago Supernova Catalogue 1999 The Asiago Supernova Catalogue - 10 years after R Barbon V Buondi E Cappellaro M Turatto Astron. Astrophys. Suppl. Ser. 139 531 1999 1999A&AS..139..531B II/218 : Sternberg Supernova Catalogue (Tsvetkov+ 1998) Supernovae Surveys supernovae and supernovae remnants: general galaxies: general galaxies: stellar contents Ten years after the publication of the previous release, we present a new edition of the Asiago Supernova Catalogue updated to December 31, 1998 and containing data for 1447 supernovae and their parent galaxies. In addition to the list of the data for a large number of new SNe, we made an effort to search the literature for new information on past SNe as well. We also tried to update and homogenize the data for the parent galaxies. This catalogue supersedes the previous version <II/159>
List of SNe arranged in chronological order n_SN *: Occurrence of multiple SN discoveries in the same galaxy --- SN Supernova designation --- u_SN ?: Unconfirmed SN --- Galaxy Parent galaxy identification --- RAgh Parent galaxy right ascension (J2000) h RAgm Parent galaxy right ascension (J2000) min RAgs Parent galaxy right ascension (J2000) s u_RAgs Uncertainty flag when RAg=hhmm.m --- DEg- Parent galaxy declination sign (J2000) --- DEgd Parent galaxy declination (J2000) deg DEgm Parent galaxy declination (J2000) arcmin DEgs Paretn galaxy declination (J2000) arcsec RAh Supernova right ascension (J2000) h RAm Supernova right ascension (J2000) min RAs Supernova right ascension (J2000) s DE- Supernova declination sign (J200) --- DEd Supernova declination (J2000) deg DEm Supernova declination (J2000) arcmin DEs Supernova declination (J2000) arcsec u_DEs Uncertainty flag when DE=-ddmm.m --- MType Parent galaxy morphological type --- MTypeC Parent galaxy morphological type code --- Incl Only for disk-like system, inclination of the polar axis with respect to the line of sight ($0$ for face on systems) deg PA Position angle of the major axis of the parent galaxy (North Eastwards) deg HRV Parent galaxy heliocentric radial velocity km/s u_HRV Uncertainty flag on HRV --- z Redshift for objects with redshift z>=0.1 --- u_z Uncertainty flag on z --- n_Bmag Prefix for photographic magnitudes --- Bmag Parent galaxy integrated B magnitude mag logD25 Decimal logarithm of the apparent isophotal diameter [0.1arcmin] x SN offset from the galaxy nucleus, in the E/W direction arcsec n_x Orientation of x number=1 For 1992ak, in the original discovery report they forgot to give the direction of the offset, so and n_x was set to ?. --- y SN offset from the galaxy nucleus, in the N/S direction arcsec n_y Orientation of y --- Com CC: close center; NC: near center --- Band SN magnitude band --- MaxMag If available, supernova magnitude at maximum (photometric band indicated) --- u_MaxMag Uncertainty flag on MaxMag --- n_MaxMag *: discovery magnitude r: radio --- Type Supernova type --- EpMax If known, date of maximum --- n_EpMax *: Date of discovery --- Disc Name(s) of discoverer(s) --- Patricia Bauer CDS 1999 Sep 20 Enrico Cappellaro <cappellaro@pd.astro.it> II_227.xml The Stromgren and Perry Photoelectric uvby Catalog 2901 II/901 ubvy Photometry of Stars Brighter than V=6.5mag The Stromgren and Perry Photoelectric uvby Catalog B Stromgren C L Perry unpublished ??? ??? 1965 1965 Photometry, uvby The catalog contains photoelectric uvby photometry for 1217 stars brighter than V=6.5 magnitude, mostly of spectral classes A, F, and G. The uvby colors allow the determination of both spectral type A2 - G2 stars and the relative metal abundance for late F- and early G-type stars. The measurements were made with telescopes of 16 to 36 inches at Mount Palomar and Kitt Peak Observatories. The catalog includes star names, right ascension and declination (B1950); V magnitudes; the color indices b-y, m1, c1; spectral types, and cross numbering systems of the Bright Star catalogue, the Henry Draper Catalogue, and the Durchmusterung catalogs.
The photometric data ID Stromgren and Perry sequential Number --- name1 Star name 1 - Flamsteed number --- name2 constellation abbreviation --- HR Yale Bright Star number (Harv. Revised) --- RAh Right Ascension (1950.0) hours h RAm Right Ascension (1950.0) minutes min DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin V1 Visual Magnitude based on this cat. mag b-y b-y Color Index A color index that is relatively insensitive to chemical-composition effects. mag m1 m1 Color Difference = (v-b) - (b-y) A color difference that is a measure of the total intensity of the metal lines in the v band. mag c1- Sign of c1 (see next field) --- c1 c1 Color Difference = (u-v) - (v-b) A color difference that is a measure of the Balmer discontinuity. mag NumObs Number of individual observations --- HD Henry Draper number --- DMsign sign of Durchmusterung number --- DMzone zone of Durchmusterung number --- DM sequential number within zone --- V2 Visual Magnitude based on Yale BS Cat. 0.01mag B-V- sign of B-V color --- B-V B-V color (from the Yale BS Cat.) 0.01mag Sp Spectral type If composite spectral class, there is a plus sign "+" in byte 117. --- C.-H. Lyu Hughes STX/NASA Julie Anne Watko SSDOO/ADC 1996 Mar 08 The original ADC documentation by Theresa A. Nagy and Robert S. Hill (1981) was used to create this ReadMe file. UNKNOWN UNKNOWN The Stromgren and Perry Photoelectric Catalogue was made machine-readable at NASA/Goddard Space Flight Center in the early 1970s. Since this catalogue has the Yale Bright Star Catalogue number (HR= Harvard Revised), some selected data has been added from the latter in particular the two identifiers: Henry Draper number and Durchmusterung number; the magnitude information V (typically to 0.01m as opposed to 0.1m from the Stromgren and Perry Catalogue), the B-V color; and all of the spectral type information from the Yale Bright Star Catalogue. II_901.xml Preliminary General Catalogue of Early-Type Emission Stars 3002 III/2 Preliminary General Cat Early-Type Emission Stars Preliminary General Catalogue of Early-Type Emission Stars F C Bertiau M F S J McCarthy Ricerche Astron. 7 523 1969 1969RA......7..523B Stars, emission Stars, Be The present catalogue presents a list of 3216 stars mostly earlier than type F which have shown emission features and specifically one or more lines of the Balmer series in emission. It is a compilation and rearrangement of the following lists: the Catalogue and Bibliography of Stars of Classes B and A whose spectra have bright H lines by P. Merrill and C. Burwell, the lists of Haro and his associates at Tonantzintla, the catalogues of Luminous Stars in the Northern Milky Way, Vols. I to VI published by the astronomers of the Hamburger Sternwarte and the Warner and Swasey Obs. Shorter lists of emission stars published by Parenago, Bidelman and McCarthy and Treanor have also been included. The present catalogue has a simple aim: to assist the astronomer in finding from a vast array of articles in the literature whether the star under investigation has been known to show emission features in the earlier major surveys of emission stars of early type carried out at the Mount Wilson, Tonantzila, Hamburg and Warner-Swasey Observatories. The catalogue includes the star identification, Durchmusterung identification, source catalog, RA and Dec, Galactic latitude and longitude, apparent magnitude, spectral classification and remarks.
Data ID Vatican Serial Number. --- n_ID 'M' for Multiple Entry M = same star is listed in multiple sources first source only is given in ref see Table three in the original publication for additional references * = uncertain identification of stars in different sources stars and sources are listed on separate records --- DM_cat Durchmusterung Catalog: BD, CD or HD --- DM Durchmusterung Identification The rubric that was adopted in the Henry Draper Catalogue of denoting declinations different from the declination of the 1900.0 epoch has been followed in the present catalogue. For example, Vatican No. 7 which is the equivalent of Star No. 3 in the A catalogue (i.e. Merrill and Burwell: Mount Wilson Catalogue, Star No. 3) is indicated as BD -2829 to indicate, by reference to DE (60deg, 4arcmin), that this star is BD +59 2829. Thus, the "-" denotes in this catalogue (just as the italics did in the Henry Draper Catalogue) the fact of the change in declination of the star between the 1855 epoch of the Bonner Durchmusterung and the 1900 epoch adopted for all the stars in the present listing. --- ref The Source Catalogues The source catalogues where the emission features is noted. Code letters are indicated in table1.dat For multiple sources see Table Three in the publication. () = In a few cases stars in the Luminous Star lists were cited in more than one catalogue of this series. The LS serial number listed in parentheses corresponds to the earlier catalogue. - = see Note on DM --- name The Name of the Star --- M The number in Parenago P. et al. For stars in the Orion Region, see: Parenago P. 1954, General Catalogue of Stars in Regions Investigated, Sternberg Inst. Moscow, 25. --- RAh Right Ascension (1900) hours h RAm Right Ascension (1900) minutes min DE- Declination (1900) sign --- DEd Declination (1900) degrees deg DEm Declination (1900) arcminutes arcmin mag Apparent Magnitude Apparent magnitudes as found in the original source catalogue. These are of necessity a mixture of visual magnitudes taken from various Durchmusterungs, photographic magnitudes interpolated from Selected Areas, open cluster sequences and in some cases derived directly by the various authors from visual inspection of spectrum plates. Hence very large differences in the published magnitudes for the same star are quite common even apart from the known or suspected variability of many of these stars. mag n_mag Remark on mag V = variable star * = the magnitude is markedly uncertain --- Glon Galactic longitude deg Glat Galactic latitude. deg Sp The Spectral Classification The letter "e" is omitted since presumably all stars listed have shown emission characteristics. --- n_Sp Remark on Sp C = refers to the continuous emission feature L = refers to the line emission beginning at H beta * = denotes uncertainty in the emission feature observed --- List of Source Catalogs ref Reference Code --- aut Authors If aut is blank, then some other field is continued from the previous line. --- ent Entries --- bib Reference --- Ep Epoch a rem Remarks on Magnitude Systems Remarks on Magnitudes Listed in Catalogue 1. Visual Magnitudes except where Marked. 2. Mostly Photographic Magnitudes. 3. Magnitudes Not Listed. 4. Provisional Photographic Magnitudes. 5. Visual Magnitudes. 6. Photographic Magnitudes. 7. Photographic Magnitudes except where Marked. 8. Approximate Photographic Densities estimated from Spectra and converted into Magnitudes. Spectral Image Densities based on photoelectric sequences. 9. Iris Photometer Readings on direct Plates calibrated by photoelectric sequences. 10. Photoelectric B Magnitudes. --- Julie Anne Watko SSDOO/ADC 1996 May 07 III_2.xml Studies of the Milky Way from Centaurus to Norma III. OB Stars 3006A III/6A Milky Way Studies, Centaurus to Norma. III. OB Stars Studies of the Milky Way from Centaurus to Norma III. OB Stars G Lynga Medd. Lund, Ser. II, No. 141 ??? ??? 1964 1964MeLu2.141....1L Milky Way Stars, OB Regional catalog This catalog is survey of OB stars in the Southern Milky Way done as part of work performed from 1961-963 at the Uppsala Southern Station at Mount Stromlo. Objective prism plates from a 50/65cm Schmidt telescope were searched for faint OB stars between galactic longitudes lII=310 degrees and lII=334 degrees, resulting in a catalog of 483 objects. The data file contains a running number, CD, CPD, HD numbers, RA and Dec (1950.0), magnitude from CD or CPD, ptm magnitude and spectral class from HD.
Main data file num Running sequence number --- CPDzone CPD zone Follows convention of AD catalog, i.e. for stars whose declination in 1875 was north of -52 degrees, the CD was used. For stars south of this limit the CPD was used. If a star was not found in the appropriate catalog, but was present in the other, the number from the other was used. A total of 55 stars were not present in either catalog. Their coordinates were estimated from the direct plates taken with the Uppsala Schmidt telescope, using plots of CD or CPD stars to an accuracy of about 1 arcminute. --- CPDnum CPD number --- CDzone CD zone number --- CDnum CD number --- HD HD number --- RAh Right ascension hours (1950.0) h RAm Right ascension minutes (1950.0) min RAs Right ascension seconds (1950.0) s DE- Declination sign (1950.0) --- DEd Declination degrees (1950.0) deg DEmin Declination minutes (1950.0) arcmin CPDmag Magnitude from CPD or CD catalog 0.1mag ptm Ptm magnitude from HD catalog 0.1mag Sp Spectral class from HD catalog --- James E. Gass SSDOO/ADC 1997 Sep 15 III_6A.xml A Survey of Faint OB Stars in Carina 3007A III/7A Survey of Faint OB Stars in Carina A Survey of Faint OB Stars in Carina J A Graham G Lynga Mem. Mt. Stromlo Obs. 18 ??? ??? 1965 1965MmMtS..18.....G Stars, hot MK spectral classification A finding list is presented for OB stars in a 75 square degree region centered on eta Carina. Completeness between 8.5 and 11.5 was the goal. Crowding, rather than the plate limit determined the limiting magnitude. The catalog contains HD, HDE, or CPD numbers, positions, visual magnitudes, HDE types, and numbers in the Tonantzintla Bulletins when available.
The spectral types were estimated from eight Uppsala Schmidt plates. The magnitudes may be rough but were estimated against both photographic and photoelectric sequences.
The finding list ID Running number --- CPDz CPD zone --- CPDn CPD number --- HD HD or HDE number --- RAh Right ascension hours (1975.0) h RAm Right ascension minutes (1975.0) min RAs Right ascension seconds (1975.0) s DE- Declination sign --- DEd Declination degrees (1975.0) deg DEm Declination minutes (1975.0) arcmin m-v Visual magnitude mag sp HDE type --- Nancy Grace Roman ADC/SSDOO 1996 Sep 06 III_7A.xml F2-G5 Stars in a North Galactic Pole Region 3009A III/9A F2-G5 Stars in a North Galactic Pole Region F2-G5 Stars in a North Galactic Pole Region A R Upgren Jr. Astron. J 68 194 1963 1963AJ.....68..194U Galactic pole, north Regional catalog The catalog is an objective-prism survey for stars of spectral classes F2 to G5 in a region of high galactic latitude. The catalog contains 1127 stars and is complete to a limiting photographic magnitude of 12.5. The photographic plates used permit a separation of the stars into narrow and well-defined spectral classes. The spectral classification of the stars in the catalog is based on the Yerkes MK system. The catalog is subdivided into one-degree declination zones as are the DM catalogs. The degree zones are based on 1855 coordinates. The catalog includes sequence numbers of the stars, BD and HD numbers, positions (B1950), B magnitudes, spectral types, and remarks.
catalog data UI UI number --- BD BD number --- HD HD number --- RAh Right ascension, equinox 1950, hours h RAm RA minutes min DE- sign of DEC --- DEd Declination, equinox 1950.0, degrees deg DEm Dec arcminutes. arcmin B B magnitude. There is a <Null> value in column 'B' on line 1054 of which UI number is 41 101. This star is observed on two deep plates, 4765 and 5471, taken over one year apart, to be of spectral classes F2 and A5, respectively, and magnitudes 12.6 and 12.1, respectively, and is not included in the list by Slettebak and Stock (1959). The A5 spectral image appears similar to one of RR Lyrae of the same dispersion (Nassau and Stephenson 1960). It is likely that this star is a previously undiscovered RR Lyrae type variable. --- Sp Spectral type --- u_Sp uncertainty in Sp --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 10 III_9A.xml G5 and Later Stars in a North Galactic Pole Region 3010A III/10A G5 and Later Stars in a North Galactic Pole Region G5 and Later Stars in a North Galactic Pole Region A R Upgren Jr. Astron. J. 67 37 1962 1962AJ.....67...37U Galactic pole, north Regional catalog The catalog is an objective-prism survey of late-type stars in a region of 396 square degrees surrounding the north galactic pole. The objective-prism spectra employed have a dispersion of 580 A/mm at H-gamma and extend into the ultraviolet region. The catalog contains the magnitudes and spectral classes of 4027 stars of class G5 and later, complete to a limiting photographic magnitude of 13.0. The spectral classification of the stars is based on the Yerkes system. The catalog includes the serial numbers of the stars corresponding to the numbers on the identification charts, BD and HD numbers, B magnitudes, spectral classes, and letters designating the subregion and identification chart on which each star is located. This survey was undertaken to determine the space densities at varying distances from the galactic plane. Accurate separation of the surveyed stars of G5 and later into giants and dwarfs was achieved through the use of the uv region as well as conventional methods of classification. The resulting catalog of 4027 stars is probably complete over the region to a limiting photographic magnitude of 13.0. The region covered by the survey is the same as that discussed by Slettebak and Stock (1959, A Finding List of Stars of Spectral Type F2 and Earlier in a North Galactic Pole Region, Hamburger Sternwarte) and is in the approximate range RA 11 30 to 13, Declination +25 to +50 (B1950.0). The catalog includes all M and Carbon stars previously published by Upgren (1960, Astron. J. 65, 644). For a discussion of the classification criteria, the combining of multiple classifications (each spectral image was classified twice), the determination of magnitudes, and additional details about the catalog, the source reference should be consulted.
Catalog data zone Zone designation --- Starnum Star number (sequential) --- DM_z BD zone --- DM_n BD number --- HD HD number --- Mag Magnitude mag Sp Spectral type (colons for uncertainty) --- Region Region --- flag Note flag (asterisk) --- Notes for this catalog Cat1 Catalog number part I --- Cat2 Catalog number part II --- rem Remarks --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 10 UNKNOWN UNKNOWN The catalog, as originally received by the Centre de Donnees Astronomiques de Strasbourg, was essentially in the form of the published table, but with a brief data description (by columns) in free text at the top of the file. However, some kind of strange pseudo-coordinates had been added to the records. Right ascensions for each region started at some value and increased by 0.01 hours for each succeeding star. From each right ascension and the declination zone (only), galactic coordinates had been computed. The right ascensions then restarted for each new region. The source of these coordinates is unknown, as they were not in the original catalog; Dr. Upgren did not computerize the machine version and had no knowledge of their existence. These coordinates were removed at the ADC. A comparison of the machine-readable file against the published catalog also revealed a number of errors, such as duplicate and missing records. A number of errors had also been discovered by Dr. S. Nishimura of the Japanese Astronomical Data Center, National Astronomical Observatory, Tokyo. The errors have been corrected in the present file. The notes to the catalog were computerized at the ADC and are flagged by asterisks in the main file. III_10A.xml F2 and Earlier Stars in S.A. 28, 54, 106, 107 3011A III/11A F2 and Earlier Stars in SA28, 54, 106, 107 F2 and Earlier Stars in S.A. 28, 54, 106, 107 A R Upgren Jr. R T Staron Astrophys. J. 157 327 1969 1969ApJ...157..327U Selected areas The catalog contains the results of an objective-prism survey for 498 stars of spectral classes F2 and earlier, brighter than magnitude 11.5, in four regions of intermediate galactic latitude. This objective-prism survey is part of a study of stellar densities aiming at the determination of the inclination to the galactic plane of surfaces of equal stellar density. Each region is centered on one of the Selected Areas 28, 54, 106, and 107. The fields, 4 x 4 degrees in size, were each photographed on two IIa-O emulsion plates, one with an exposure time of three minutes on which bright stars could be classified and one with an exposure time of 40 minutes extending to faint stars. The plates were taken with the 24-inch Baker-Schmidt telescope of the Dyer Observatory. The dispersion of the objective prism is about 330 A/mm at H-gamma. The stars were classified according to the criteria established by Nassau and Seyfert (1946) and Nassau and van Albada (1947). Photographic magnitudes were found from direct IIa-O plates taken with the eight-inch Ross camera of the Yale Observatory. The catalog includes BD numbers, magnitudes, and spectral classes for BD stars. For non BD stars, the BD number listed in column (1) indicates a nearby BD star from which the star listed is offset, as indicated by the data of columns (2) and (3).
BD stars catalog data Sarea Selected Area number --- BD BD number --- Photomag Photographic magnitude mag Sp Spectral type --- u_Sp uncertainty in Sp --- Non-BD stars Sarea Selected Area number --- BD BD number of nearby star --- RAoffset Right ascension offset from BD star given in bytes 5-12, minutes of arc arcmin DEoffset Declination offset from BD star given in bytes 5-12, minutes of arc arcmin Photomag Photographic magnitude mag Sp Spectral type --- u_Sp uncertainty in Sp --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 10 UNKNOWN UNKNOWN Data format modified at the Astronomical Data Center (ADC)/NASA GSFC, 1988 June...WHW III_11A.xml F5 and Later Stars in Selected Areas 28, 54, 106, 107 3012A III/12A F5 and Later Stars in SA28, 54, 106, 107 F5 and Later Stars in Selected Areas 28, 54, 106, 107 A R Upgren Jr. R T Staron Astrophys. J. Suppl. 19 367 1970 1970ApJS...19..367U Selected areas The catalog is an objective-prism survey of 2181 stars later than spectral class F2; the earlier stars are in catalog ADC# 3011A. The limiting magnitude is about 11.5. Four regions of intermediate galactic latitude are included in this survey. Each region is centered on one of the Selected Areas 28, 54, 106, and 107 and consists of a square 7 degrees on a side or about 50 square degrees in area. The fields, 4 x 4 degrees in size, were each photographed on two IIa-O emulsion plates, one with an exposure time of three minutes on which bright stars could be classified and one with an exposure time of 40 minutes extending to faint stars. The plates were taken with the 24-inch Baker-Schmidt telescope of the Dyer Observatory. The dispersion of the objective prism is about 330 A/mm at H-gamma. The stars were classified according to the criteria established by Nassau and Seyfert (1946) and Nassau and van Albada (1947). Photographic magnitudes were found from direct IIa-O plates taken with the 8-inch Ross camera of the Yale University Observatory. The catalog includes BD numbers, magnitudes, and spectral classes for BD stars. For non BD stars, the BD number listed in bytes 1-3 indicates a nearby BD star from which the star listed is offset by the values in bytes 5-12 and 15-17 given in minutes of arc.
catalog data for BD stars AreaNum Selected Area number --- BD BD number --- PhotoMag Photographic magnitude mag u_PhotoMag Colon for uncertainty in photographic magnitude --- SpTemp Spectral type, temperature class and subclass --- u_SpTemp Colon for uncertainty in temperature class/subclass --- LumCl luminosity class --- u_LumCl Colon for uncertainty in luminosity class --- data for non-BD stars AreaNum Selected Area number --- BD BD number of nearby star --- RAoffset Right ascension offset from BD star given in bytes 5-12, minutes of arc arcmin DEoffset Declination offset from BD star given in bytes 5-12, minutes of arc arcmin PhotoMag Photographic magnitude mag u_PhotoMag Colon for uncertainty in photographic magnitude --- SpTemp Spectral type, temperature class and subclass --- u_SpTemp Colon for uncertainty in temperature class/subclass --- LumCl luminosity class --- u_LumCl Colon for uncertainty in luminosity class --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 10 UNKNOWN UNKNOWN This survey is part of a study of stellar densities with a view toward determining the inclination to the galactic plane of surfaces of equal stellar density. Data format modified at the Astronomical Data Center (ADC)/NASA GSFC, 1988 June...WHW III_12A.xml Vyssotsky's Catalogues 1950.0 3013 III/13 Vyssotsky's Catalogues 1950.0 Vyssotsky's Catalogues 1950.0 A N Vyssotsky Astrophys. J. 97 381 1943 1943ApJ....97..381V Vyssotsky's Catalogues 1950.0 A N Vyssotsky E M Janssen N J Miller S J Walther M E Walther Astrophys. J. 104 234 1946 1946ApJ...104..234V Vyssotsky's Catalogues 1950.0 A N Vyssotsky B A Mateer Astrophys. J. 116 117 1952 1952ApJ...116..117V Vyssotsky's Catalogues 1950.0 A N Vyssotsky Astron. J. 61 201 1956 1956AJ.....61..201V Vyssotsky's Catalogues 1950.0 A N Vyssotsky Astron. J. 63 211 1958 1958AJ.....63..211V Spectral types Space velocities This catalog includes the results of a complete survey of the McCormick prismatic spectral plates for M dwarf stars. catalog.dat includes identifications, magnitudes, proper motions in RA and Dec, spectral types and parallaxes.
Catalog ID Star number --- zone BD or AC zone deg num BD or AC number --- RAh Right ascension hours (1950) h RAm Right ascension minutes (1950) min DE- Sign of declination --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin magv Visual magnitude mag pmRA Proper motion in right ascension arcsec pmDE Proper motion in declination arcsec Sp Spectral type --- n_Sp Suffix for peculiar or emission --- Plx Parallax arcsec Julie Anne Watko and N. G. Roman SSDOO/ADC 1997 Nov 06 III_13.xml A Finding List of Stars F2 and Earlier in a North Galactic Pole Region 3014A III/14A F2 and Earlier Stars, North Galactic Pole Region A Finding List of Stars F2 and Earlier in a North Galactic Pole Region A Slettebak J Stock Hamburger Sternwarte 5, No. 5 ??? ??? 1959 1959AAHam...5..105S Galactic pole, north The catalog is the result of an objective-prism survey made with the Hamburg 80-cm/120-cm Schmidt telescope. The F2 and earlier stars were isolated from later-type objects by using the MK classification criteria discussed in the source reference. The catalog contains 601 stars and includes cross identifications to the numbering systems of the BD and HD catalogs, coordinates (equinox B1950.0), photographic magnitudes, and spectral types. The catalog consists of three files. The first two files contain data. File 1 is for BD stars and File 2 is for non-BD stars. File 3 contains the remarks from the original data tables merged with those following the data.
BD Stars Non-BD Stars Num Running number used on the charts in the published paper --- BD BD number The sign is always in byte 4, the zone in bytes 5-6, and the number in bytes 7-10. All stars in bdstars.dat have BD numbers. This field is always blank for the non-BD stars in nonbd.dat. --- HD Number in the Henry Draper (HD) Catalogue. Blank if star has no HD and always blank in nonbd.dat --- RAh Right ascension for equinox 1950 (in hours) h RAm R.A. (minutes) min DE- Declination for equinox 1950. --- DEd DEC (degrees) deg DEm Dec. (arcminutes) arcmin Photomag Photographic magnitude from HD or AGK2 catalogues or estimated from prints of the original plates by comparison with standard stars from Selected Areas. Intended for identification purposes only. mag Sp Spectral classification. Mt. Wilson luminosity classes in bytes 33-34. A temperature class (A, F) is always in byte 35, but temperature subclasses and peculiarities are not uniform within the data field. --- flag An asterisk if there is a note in the remarks file; otherwise blank. --- Notes StarNum Star number in the data catalog. --- flag "B" if the star belongs to the BD file, "N" if to the non-BD file. --- RemNum Integer used to sequentially number remarks for the same star. Can be used alone or with byte 4 as a sort field for reordering the remarks properly if they become disorganized. --- rem Remarks in upper and lower case characters --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 22 UNKNOWN UNKNOWN The data set A Finding List of Stars of Spectral Type F2 and Earlier in a North Galactic Pole Region was received from the Centre de Donnees Stellaires, Strasbourg. As received, the data were contained in a single file with 626 logical records of length 80 bytes. Each data table was preceded by a brief title and data explanation and the notes were not included. The following modifications were made to produce the three-file catalogue described here: 1. The single file was divided into two files, one for the BD stars and one for the non-BD stars, as the tables are separate in the original publication. All but the data records were deleted, since explanatory material of greater detail is now contained in the document. 2. From a record count and comparison with the published paper, two missing records were discovered. These were added to the files. Ampersands (from BCD coding) were changed to plus signs on all BD numbers and declination values. 3. The spectral-type field was moved and made more uniform by shifting types so that a temperature class is always in byte 35. 4. Information from the "Remarks" columns in the published tables and the notes to the tables was combined, computerized and added as a third file. For each star having a remark or remarks in the notes file, an asterisk (*) was added to byte 42 of its record in the data files. 5. The logical record length of both data files was shortened from 80 bytes to 42 bytes since bytes 43-80 were never used. III_14A.xml Catalogue of Early-Type Stars Whose Spectra Have Shown Emission Lines 3017B III/17B Early-Type Emission-Line Stars Catalogue of Early-Type Stars Whose Spectra Have Shown Emission Lines L R Wackerling Mem. Roy. Astron. Soc. 73 153 1970 1970MmRAS..73..153W Stars, emission Stars, early-type Stars, Be The catalog contains 5326 early-type emission-line stars. Of these, 1424 have no spectral classification but are assumed to be of early type. Some 71 percent of the stars listed here can also be found in the Mount Wilson and the Mount Wilson-Michigan survey catalogs. The catalog contains numerous cross identifications to other designations (name, HD, DM, LS, MWC, TON, HIL, WRA, HEN, etc.), spectroscopic type, magnitudes (visual and blue), equatorial (B1900 and B1950), and galactic coordinates.
Wackerling's catalogue Cntr Sequential counter based on order in RA(1900) --- Name Common name of the object --- u_Name ':' if Name in uncertain --- ID_Codes Usually one of the IDs from the indiv. cats. --- HD Henry Draper Catalog (HD) number --- m_HD HD Component, or ':' if uncertain --- DM Durchmusterung catalog number 'BD', 'CD', 'CP' --- m_DM DM component, or ':' if uncertain --- MWC Mt. Wilson Cat. (MWC) or Add. Stars (AS) number --- u_MWC ':' if the MWC identification is uncertain --- HPC Hiltner Polarization Catalogue number --- u_HPC ':' if HPC identification is uncertain --- Ton Tonontzintla number, see ADC document --- LS Luminous Stars number, see ADC document --- m_LS Luminous Star component, or ':' if uncertain --- Wray Number from J.D. Wray emission-line star list --- u_Wray ':' if the Wray identification is uncertain --- Henize Number from Henize emission-line star list --- u_Henize ':' if the Henize identification is uncertain --- RA1900h Hours RA, equinox B1900.0 h RA1900m Minutes RA, equinox B1900.0 min DE1900- Sign Dec, equinox B1900.0 --- DE1900d Degrees Dec, equinox B1900.0 deg DE1900m Minutes Dec, equinox B1900.0 arcmin RAh Hours RA, equinox B1950.0 h RAm Minutes RA, equinox B1950.0 min DE- Sign Dec, equinox B1950.0 --- DEd Degrees Dec, equinox B1950.0 deg DEm Minutes Dec, equinox B1950.0 arcmin PrecRA Precession in RA, 50 yr from 1950 to 2000 min PrecDec Precession in Dec, 50 yr from 1950 to 2000 arcmin GLON Galactic longitude deg GLAT Galactic latitude deg SpType Spectral type, see table 1 number=2 See Table 1 for the main codes; see emline.doc for further details -------------------------------------------------------------------------------- Table l. Spectral Type Codes Type Code Category --------- -------- OB OB group O, B, A, F of unknown luminosity class O, B, A, F * of MK Class III, IV or V CO, CB, CA, CF * of MK Class I or II OF Of WR, WC, WN, WP (3)Wolf-Rayet SB subluminous B UG U Gem or Z Cam Q old nova RQ recurrent nova X identified with an X-ray source Z symbiotic CQ super luminous nova-like variable BQ, AQ, FQ shell component present in spectra Y (1)central star of a planetary nebulae + (2)binary star --- Vmag Apparent visual magnitude number=1 the photoelectric magnitude of Wolf-Rayet stars is the Smith-Westerlund v or b magnitude when available. mag n_Vmag '*' for photoelectric, 'V' for variable --- Bmag Apparent blue magnitude number=1 the photoelectric magnitude of Wolf-Rayet stars is the Smith-Westerlund v or b magnitude when available. mag n_Bmag '*' for photoelectric, 'V' for variable --- emline.doc ADC Documentation by T.A. Nagy and R.S. Hill Toshihiro Horaguchi Japan 1996 Feb 06 III_17B.xml Catalogue of Stellar Spectra Classified in the Morgan-Keenan System 3018B III/18B Stellar Spectra Classified in Morgan-Keenan System Catalogue of Stellar Spectra Classified in the Morgan-Keenan System C Jaschek H Conde A C de Sierra Publ. La Plata Obs., Ser. Astron. 28, No. 2 ??? ??? 1964 1964PLPla..28....1J MK spectral classification Spectral types The purpose of this catalog is to provide bibliographic references to spectral classifications of stars in the Morgan-Keenan system published in the literature prior to January 1963. The catalog includes, with few exceptions, only objects contained in the Durchmusterungen: BD, SD, CD, and CPD. Objects belonging to stellar clusters and extragalactic nebulae were excluded from the catalog if they are not listed in the Durchmusterungen. The catalog includes sequential numbers, HD and DM numbers, right ascension and declination (B1900.0), magnitudes, spectral classifications, and bibliographic references. This machine-readable version was modified and corrected with errata at the Astronomical Data Center/Goddard Space Flight Center, NASA/Goddard Space Flight Center.
Catalog Data count Counter within a group of records For any given star there may be as many as 11 records. The first record of such a group gives a spectral classification and references, while subsequent records may be used merely to continue the list of references which gave that classification, or subsequent records are used to give different classifications (and associated references) for the given star. --- HD HD number --- n_HD Additional designation or alternate number --- DM_cat DM catalog designation --- DM_sign Sign of DM zone --- DM_zone Declination zone deg DM_num Number within zone --- n_DM Additional designation --- name Alternative name --- RAh Right ascension hours (1900.0) h RAm Right ascension minutes (1900.0) min DE- Sign of declination --- DEd Declination degrees (1900.0) deg DEm Declination minutes (1900.0) arcmin mag Magnitude (accuracy is uncertain) For identification purposes only Two stars have non-digits in the magnitude field. GM Per (line 3704) has the magnitude 9.0) HD 38268 (line 5015) has NEB in the magnitude column mag Sp Spectral type Peculiar objects are generally included; subdwarfs listed occasionally; N, R, and S stars usually mentioned; white dwarfs omitted. --- note References and notes Each reference is given as a three digit integer followed by a blank. The notes are coded as follows: V variable SB spectroscopic binary VB visual binary TS triple system --- com Asterisk indicates corrected value --- RAr Right ascension in radians rad DEr Declination in radians rad cnt Counter from hard copy catalog A counter which sequentially numbers the entries in the hardcopy. The records in the machine readable version have been reordered by right ascension (1900). --- mkclass.txt *The original ADC document The file summary, format description, and changes have been removed as they are included in either the ReadMe or changes.txt changes.txt Changes made by ADC N.G. Roman ADC/SSDOO 1997 Aug 07 III_18B.xml Rotation of Evolving A and F Stars 3022 III/22 Rotation of Evolving A and F Stars Rotation of Evolving A and F Stars I J Danziger S M Faber Astron. Astrophys. 18 428 1972 1972A&A....18..428D Rotational velocities Stars, A-type Stars, F-type The authors have studied a vertical strip in the HR diagram covering the range of spectral types A5 through F9. Rotational velocities for a total of 579 stars of all luminosity classes were accumulated. HR number, rotational velocity v sin(i), (b-y) index, m1, c1, reference and group are given.
Approximately 360 stars from the Bright Star Catalogue (Hoffleit, 1964) were observed with the coude spectrograph on the 84 in. telescope at Kitt Peak National Observatory at a dispersion of 13.6 A/mm. A few stars were observed with the coude spectrograph on the 100 in. telescope at Mt. Wilson. The re- mainder were obtained from the published material that the authors considered to provide reliable rotational velocities. The values given here generally agree with the mean v sin(i) found in the literature to within 15%. The method for determining the rotational velocities is somewhat different from the usual approach. A grid of standard stars, judged from their line-widths to have small rotation, was chosen. Five sections of their spectra traced on the microphotometer at Harvard College Observatory were mathematically broadened according to the usual formula to provide a grid of spectra with which observed spectra could be compared to obtain the rotational velocity.
Rotational Velocities and Photometric Data HR Number in the Yale Catalogue of Bright Stars (Hoffleit D., 1964) --- vsin(i) Rotational Velocity v sin(i) for HR 3889 was given as "175,30*" in published catalog. v sin(i) for HR 3936 was given as " 90,30*". These values in this file are blank. km/s b-y (b-y) index mag m1 m1 (v-b) - (b-y) fr˜h (U,v,b,y) mag c1 c1 = (u-v) - (v-b) J mag ref Source of photometric data 1 = Stromgren B. & Perry C.L. (1962) 2 = Breger M. (1969) When no source is given, the data were obtained by the authors. --- group Group The main-sequence band was subdivided into six groups (A to F), each occupying a specific area in the HR diagram. (see Fig. 3 in the original paper) --- Julie Anne Watko SSDOO/ADC 1996 May 30 III_22.xml MK Classification for OB Stars 3023B III/23B MK Classification for OB Stars MK Classification for OB Stars J R Lesh ApJS 17 371 1968 1968ApJS...17..371L MK spectral classification Stars, OB Spectral types The catalog is a compilation of MK spectral types published in the paper, "The kinematics of the Gould Belt: An Expanding Group?" (Rountree Lesh 1968). Spectral types were determined for 464 stars of Henry Draper type B5 and earlier, brighter than 6.5 visual magnitude and higher than -20 degrees in declination. The spectra were classified by the author using plates taken with the Yerkes 40-inch refractor and MK spectrograph. The catalog contains HR, HD numbers, MK types with temperature classes, subclasses, luminosity classes and peculiarities, and remarks.
Catalog Data HR BS = HR number BS = HR number is the number from the Yale Catalogue of Bright Stars (Hoffleit 1964). --- HD HD number Number from The Henry Draper Catalogue (Cannon and Pickering 1918-1924) --- MKtype1 Temperature class and subclass (MK type) Spectral type classified in the MK system. --- MKtype2 Luminosity, peculiarities, etc. (MK type) Spectral type classified in the MK system. Peculiarity codes include a new classification scheme for the Be stars, assignment having been made based upon the emission lines subsequent to MK spectral type and luminosity class assignment based on absorption lines alone. The following notation is used for the emission parameter: e1 No overt hydrogen emission. Prototypes 66 Oph, 1H Cam. The H-beta absorption line is partially or completely filled in, but is not reversed. H-gamma may also show some filling in. The Fe II lines are usually absent. e1+ Prototype 48 Per. H-beta has a narrow emission core while remaining predominantly an absorption line. e2 H-beta in emission. Prototypes psi Per, 120 Tau. H-beta is an emission line. H-gamma is also filled in but is not reversed, while the other Balmer lines are not affected. The Fe II lines are often, but not always, present. e2+ Prototype HD 45995. H-gamma shows a narrow emission core and the higher Balmer lines are slightly filled in. The Fe II lines are usually rather marked. e3 Complete hydrogen emission spectrum. Prototypes 11 Cam, HD 58050. H-beta is an emission line and the higher Balmer lines, at least through H-epsilon, have emission cores. The Fe II lines are usually present, except in the earliest spectral types, but they do not dominate the spectrum. e3+ Prototype HD 41335. The Fe II lines are more prominent than at e3, but the hydrogen emission strength is less than at e4. e4 The extreme Be stars. Prototype chi Oph. There is intense emission in all the Balmer lines, plus very strong Fe II lines (except in the earliest types). This group is similar to the Bex class discussed by Schild (1966). --- flag Remarks flag An asterisk (*) denotes that remarks are present in data2.dat of the catalog. --- Remarks HD HD number HD number of the star in The Henry Draper Catalogue (Cannon and Pickering 1918-1924) --- rem Remarks Remarks in free text (upper and lower case) form. When bytes 1-6 are blank, this record continues the remarks for the previous star. --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 22 UNKNOWN UNKNOWN The machine-readable table MK Classification of OB Stars was received from the Centre de Donnees Astronomiques de Strasbourg on 5 April 1977. As received, the catalog consisted of HR numbers and spectral types with no spacing. The spectral types were recorded in all upper case characters as in the published table, except that peculiarities such as "SHELL", indicated by the notes to Table 4 in the published paper, had been added to the types themselves. The following modifications and additions to the machine-readable edition were made at the ADC: 1. Stars are identified by their HD numbers in the original publication (Rountree Lesh 1968), but the machine-readable catalog had only HR identifiers when received. A program was written to search the Yale Catalogue of Bright Stars (BSC3) (Hoffleit 1964) to retrieve HD numbers and insert them into the file. (The 1964 catalog was used because that version was cited in the MK classification work.) The same program reformatted the data to spread them a bit for improved readability. The HD numbers were proofread against the published table and an erroneous HR entry was found and corrected. One HD star not in the BSC3 had been omitted from the machine version -- it was added. 2. The spectral-type notation was modified to upper and lower case to match the standard notation. All spectral types were proofread against the published table and corrections were made so that the information agrees exactly. 3. The notes to Table 4 of the published paper were keyed into a file and added to the machine version. Asterisk flags were added to the data file in byte 28 to indicate the presence of a remark. 4. Several duplicate records were found and eliminated. There are seven stars in the published paper whose spectral types are not given; these had been omitted in the machine version as received, but were added so that all stars in the original table (and thus discussed in the paper) are now included. III_23B.xml A Catalogue of Stellar Rotational Velocities 3030A III/30A Stellar Rotational Velocities A Catalogue of Stellar Rotational Velocities P L Bernacca M Perinotto Contrib. Oss. Asiago No. 239 ??? ??? 1970 1970CoAsi.239....1B A Catalogue of Stellar Rotational Velocities P L Bernacca M Perinotto Contrib. Oss. Asiago No. 250 ??? ??? 1971 1971CoAsi.250....1B A Catalogue of Stellar Rotational Velocities P L Bernacca M Perinotto Contrib. Oss. Asiago No. 294 ??? ??? 1973 1973CoAsi.294....1B III/63 : Revised Catalogue of Rotational Velocities (Uesugi+ 1982) Bernacca, P. L., Perinotto, M., Contributions dell' Osservatorio Astrofisico dell'Universita di Padova in Asiago No. 239 (1970), No. 250 (1971), No. 294 (1973). Rotational velocities The catalog contains 1005 main-sequence single stars; 360 spectroscopic and eclipsing binaries; 189 Be and shell stars; 243 peculiar B- and A-type stars, and 1277 supergiants, giants, and subgiants, for which v sin i has been determined from 1949 to 1970. Rotational data are essentially in the Slettebak-Kraft system. The catalog provides visual magnitudes, color indices, galactic coordinates, spectral classifications, absolute visual magnitudes, adopted rotational velocities, descriptive information, binary types, luminosity classes, orbital periods, right ascension and declination (B1900.0), and cross identifications to the numbering systems of The Henry Draper Catalogue (HD), the Durchmusterung catalogs, and Aitken Double Stars Catalogue (ADS).
Catalog Data Num Running Number --- Section Flag for Section Flag for Section 1-I Main Sequence Single Stars 2-II Main Sequence Spectroscopic Binaries & Eclipsing Systems 3-IIIa Be and Shell Stars 4-IIIb Bp, Ap, Apec and Am Stars 5-IV Evolved Stars --- HD Henry Draper Identification Number --- DM Durchmestrung (BD/CD/CPD) designation --- ADS Identification Number of Double Star Identifications (Aitkens Double Stars) --- flag2 Denotes parenthesis in hardcopy --- m_ADS Multiplicity index for Double Stars --- Ident2 Complementary identification (in clusters) --- m_Ident2 Multiplicity index for Ident2 --- Comp Component Number (Spectroscopic Binary) --- Vmag Visual Magnitude mag n_Vmag Designates that the magnitude was not determined using the UBV System --- B-V (B-V) Color Index --- U-B (U-B) Color Index --- GLON Galactic Longitude (New System, in degrees) deg GLAT Galactic Latitude (New System, in degrees) deg Dflag Designation for Dwarf Stars --- SpType Spectral type --- Subtype Spectral subtype --- LumClass Luminosity Class --- flag5 Designation that the MK System was not available. Type assigned by using colors and the spectrum-color relationship as given by Johnson (1963, Basic Astronomical Data. p. 204, Univ. of Chicago Press) --- flag6 Other Designations --- Sp.Pec Spectral Peculiarity appears in (IIIa) Section 3 only --- Mv Absolute Magnitude mag RotVel Adopted Rotational Velocity km/s e_RotVel Probable Error km/s Group Membership Open Cluster "CL" Associations "ASS" Moving Groups "GR" Streams "STR" --- Info1 Descriptive information by section Descriptive information by section - Section 1 (I) 103-111 Blank Section 2 (II) 103-105 Radial velocity variable designation ("RV" or "RV ?") Section 3 (IIIa) 103-104 Radial velocity variable designation 105-111 "SHELL" or "POLE ON" Designation Section 4 (IIIb) and Section 5 (IV) 103-111 Other Information Examples: L BO for lambda Boo SL METAL for slightly metallic RV for radial velocity variable T AU for theta Aur C SE for chi Ser D SC for delta Sct D DE for delta Del B CE for Beta Cep-type LV for Light Variable BE for Emission Lined B-type Star TSV for Two Spectra Visible Section 5 (IV) also has some additional additional cross-identification numbers which appear in these bytes --- Btype Binary Type EB - Eclipsing Binary SB - Spectroscopic Binary --- flag7 "1" or "2" with SB to designate single or double lined spectroscopic binaries respectively --- flag8 designation appears with some SB objects to designate uncertainty --- LuminC Luminosity Class numerical code: Luminosity Class numerical code - I 1 II 2 III 3 IV 4 V 5 IA 10 IB 11 IAB 12 None 99 --- Period Orbital Period (see also flag9) d flag9 designation for orbital period given in years --- Cat Catalogue Number within Section --- RAh Equatorial Coordinates (Equinox 1900.0) Right Ascension (hours) h DEd Declination (degrees) deg Info2 Descriptive information by section Blank for Sections 1, 2, 3, and 5 Section 4 (IIIb): Spectral Peculiarity or For Am stars, spectral type according to: 143-144 K-Line Lines 145-147 Hydrogen Lines 148-151 Metallic Lines --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 22 UNKNOWN UNKNOWN The machine-readable version of the Bernacca and Perinotto Catalogue of Stellar Rotational Velocities was received from the Centre de Donnees Stellaires (CDS). The original published version of this catalogue is in 5 parts: 1. I-- Main sequence single stars 2. II-- Main sequence spectroscopic binaries and eclipsing systems 3. IIIa -- Stars with peculiar spectrum; Be and shell Stars 4. IIIb -- Stars with peculiar spectrum; Bp, Ap, Am, Apec 5. IV-- Evolved Stars The magnetic tape received from the CDS contained 2856 records but did not include section IIIb. The new total number of records is 3099. Initially the logical record length was 84 bytes, however with the added information the new logical record length is now 152 bytes. The following is a list of modifications to the CDS tape version of the BPRV Catalogue which represents the current version. 1. Section IIIb was keypunched and inserted. (Code 5 in byte 5) 2. All BD cross-identifications were keypunched and added. 3. Running counter was corrected. 4. Identification number within each section was added. 5. Equatorial coordinates (1900) were computed from the galactic coordinates as originally given on the CDS tape. 6. Missing designations that were added: a. ") " for Aitkens Double Stars . b. Type of system used in determining visual magnitude. c. Type of system used in determining luminosity class. d. 1, 2, ? with SB (Spectroscopic Binary) designation. e. RV and RV ? (RV VAR) were added to appropriate sections (II and IIIa). f. Extra information describing spectral type and luminosity class was added. (e. g., D for Dwarf). 7. A coded numbering system for luminosity class was added 8. The coordinates (Galactic and Equatorial) seem to be inconsistent. In a sample check made with coordinates from the HD Catalogue, a few sets of coordinates were found to be incorrect. We are awaiting a reply from Dr. Bernacca (Italy) to clear up this problem. Meanwhile, another tape has been made containing the BPRV records numbers that have HD numbers. This tape contains correct galactic and equatorial coordinates which were extracted and calculated, respectively, from the machine-readable version of the Henry Draper Catalogue. We are prepared to correct the coordinates on the BPRV tape if this is what is required. ADC July 1995 conversion of documentation to standard ReadMe. Verification showed several errors which could not be resolved. In records 965 and 1760 the Ident1 column had a number preceded by the letter "R". The "R" was removed but the reference is most likely to a different catalog. In record 2120 the HD number was found to be unreadable. The field only contained the value " 1 " and was modified to " 1" to comply with the format but is most likely wrong. The values for the uncertainty in the rotational velocity u_Rot_Vel in records 2489, 2574, and 2615 were not aligned "7 " was changed to " 7". III_30A.xml Michigan Catalogue of two dimensional spectral types for the HD stars. (Vol.1, -90deg < {delta} < -53deg) 3031B III/31B Michigan catalogue for the HD stars, vol. 1 Michigan Catalogue of two dimensional spectral types for the HD stars. (Vol.1, -90deg < {delta} < -53deg) N Houk A P Cowley Ann Arbor, Univ. of Michigan ??? ??? 1975 1975MSS...C01....0H III/51B : Volume 2 of this catalog (additional declination zones) III/80 : Volume 3 of this catalog (additional declination zones) III/133 : Volume 4 of this catalog (additional declination zones) MK spectra classification Plate data Spectral types This is the first of three volumes of the University of Michigan's catalogs of stellar spectral types for stars in the Henry Draper (HD) Catalog. (See catalogs 3051B and 3080 for volumes 2 and 3). It is part of a program of systematic reclassification in the MK system of the entire Henry Draper Catalogue (HD). This catalog (volume 1) includes all HD stars having declinations (1900.0) between -90 deg. and -53 deg. The stars were classified visually on objective-prism plates taken with the Michigan Curtis-Schmidt telescope at Cerro Tololo Inter-American Observatory. The 4-degree + 6-degree prisms yield a dispersion at H-gamma of 108 angstroms/mm, with a resolution of about 2 angstroms/mm, comparable to that of the original MK system. The spectra were taken on IIaO emulsion photographic plates and were widened to 0.8 mm, with exposures of 20-, 4-, and 1-min. The machine-readable catalog includes HD number, spectral type, a quality estimate, the photographic magnitude from the HD catalog, right ascension and declination (1900.0), centennial precessions, galactic coordinates, and cross identifications to the numbering systems of the HD, CD, and CPD catalogs. Separate files contain a list of the plate codes and the remarks referenced in the main catalog file.
The Catalogue, Vol.1 HD Henry Draper Catalog (HD) number --- Case '*' = sp. type lower case in printed ver. --- n_SpType '+' if spectral type is from HD Catalog --- SpType The Spectral type --- Ave_Flag 'A' if classification used is an average In this case, q_SpType is assigned the highest of the qualities used in forming the average. --- q_SpType Quality of the classification, see ADC document (adc.doc) --- Remark Remark (see adc.doc, Table 4-2) --- Ptg Photographic magnitude from HD catalog mag Var_Flag 'V' if star is known or suspected variable --- RAh Hours RA, epoch 1900.0 h RAm Minutes RA, epoch 1900.0 min DE- Sign Dec, epoch 1900.0 --- DEd Degrees Dec, epoch 1900.0 deg DEm Minutes Dec, epoch 1900.0 arcmin precRA Centennial precession in RA Very near the south pole, some of the precessions are larger than -99.9 min/century and these values are in the remarks. 0.01min/yr precDec Centennial precession in Dec 0.01arcmin/yr GLON Galactic longitude deg GLAT Galactic latitude deg CPD Cape Photographic Durchmusterung Designation 'CP' in bytes 78-79, -ZZNNNNN in bytes 80-87 --- Plate1 Plate code #1 Each plate has its own identification code (see file plates.dat) --- Plate2 Plate code #2 Each plate has its own identification code (see file plates.dat) --- Plate3 Plate code #3 Each plate has its own identification code (see file plates.dat) --- Plate4 Plate code #4 Each plate has its own identification code (see file plates.dat) --- Plate5 Plate code #5 Each plate has its own identification code (see file plates.dat) --- Remarks of Vol.1 HD Henry Draper Catalog (HD) number --- Remark Remarks in free form text --- List of Plate Codes Code Plate code --- Number Plate Number --- Date Exposure date --- adc.doc ADC Documentation Francois Ochsenbein CDS 1994 Dec 08 UNKNOWN UNKNOWN * 09-Nov-1993: list of plates added at CDS * 08-Dec-1994: list of plates corrected by Shiro Nishimura [ADAC/NAOJ] * 17-Sep-1996: brief description added by James Gass [NASA/SSDOO/ADC] III_31B.xml Ultraviolet Bright Stars Spectrophotometric Catalogue 3039A III/39A UV Bright Star Spectrophotometric Catalog Ultraviolet Bright Stars Spectrophotometric Catalogue C Jamar D Macau-Hercot A Monfils G I Thompson L Houziaux R Wilson ESA SR-27 ??? ??? 1976 1976ubss.book.....J Spectra, ultraviolet Spectrophotometry Stars, bright The catalog contains observations carried out by the S2/68 Ultraviolet Sky Survey Telescope (UVSST) aboard the ESRO Satellite, TD-1. The data presented in the catalog were obtained during the first observation period, which lasted from 19 March 1972 to 31 October 1972. The spectrum was formed on the focal surface of the spectrophotometer with a dispersion of 36 angstroms/mm. The catalog includes fluxes for each of 61 wavelengths from 1360 A to 2540 A in 20-A steps and at 2740 A, right ascension and declination (equinox B2000.0), spectral types, luminosity classes, visual magnitudes, colors, rotational velocities, references for source material, and cross identifications to the numbering system of The Henry Draper Catalogue.
TD 1A
The spectrophotometric Catalogue UVBS UV Bright Star number --- HD Henry Draper Catalog (HD) number --- Spectra Number of spectra averaged --- F1360 Flux at 1360 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1380 Flux at 1380 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1400 Flux at 1400 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1420 Flux at 1420 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1440 Flux at 1440 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1460 Flux at 1460 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1480 Flux at 1480 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1500 Flux at 1500 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1520 Flux at 1520 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1540 Flux at 1540 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1560 Flux at 1560 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1580 Flux at 1580 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1600 Flux at 1600 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1620 Flux at 1620 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1640 Flux at 1640 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1660 Flux at 1660 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1680 Flux at 1680 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1700 Flux at 1700 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1720 Flux at 1720 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1740 Flux at 1740 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1760 Flux at 1760 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1780 Flux at 1780 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1800 Flux at 1800 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1820 Flux at 1820 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1840 Flux at 1840 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1860 Flux at 1860 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1880 Flux at 1880 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1900 Flux at 1900 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1920 Flux at 1920 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1940 Flux at 1940 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1960 Flux at 1960 A (10-10erg/cm2/s/A) 10-14W/m2/nm F1980 Flux at 1980 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2000 Flux at 2000 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2020 Flux at 2020 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2040 Flux at 2040 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2060 Flux at 2060 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2080 Flux at 2080 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2100 Flux at 2100 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2120 Flux at 2120 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2140 Flux at 2140 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2160 Flux at 2160 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2180 Flux at 2180 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2200 Flux at 2200 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2220 Flux at 2220 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2240 Flux at 2240 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2260 Flux at 2260 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2280 Flux at 2280 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2300 Flux at 2300 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2320 Flux at 2320 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2340 Flux at 2340 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2360 Flux at 2360 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2380 Flux at 2380 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2400 Flux at 2400 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2420 Flux at 2420 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2440 Flux at 2440 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2460 Flux at 2460 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2480 Flux at 2480 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2500 Flux at 2500 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2520 Flux at 2520 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2540 Flux at 2540 A (10-10erg/cm2/s/A) 10-14W/m2/nm F2740 Flux at 2740 A (10-10erg/cm2/s/A) 10-14W/m2/nm e_F1360 RMS deviation of F1360 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1380 RMS deviation of F1380 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1400 RMS deviation of F1400 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1420 RMS deviation of F1420 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1440 RMS deviation of F1440 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1460 RMS deviation of F1460 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1480 RMS deviation of F1480 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1500 RMS deviation of F1500 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1520 RMS deviation of F1520 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1540 RMS deviation of F1540 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1560 RMS deviation of F1560 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1580 RMS deviation of F1580 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1600 RMS deviation of F1600 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1620 RMS deviation of F1620 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1640 RMS deviation of F1640 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1660 RMS deviation of F1660 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1680 RMS deviation of F1680 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1700 RMS deviation of F1700 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1720 RMS deviation of F1720 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1740 RMS deviation of F1740 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1760 RMS deviation of F1760 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1780 RMS deviation of F1780 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1800 RMS deviation of F1800 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1820 RMS deviation of F1820 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1840 RMS deviation of F1840 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1860 RMS deviation of F1860 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1880 RMS deviation of F1880 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1900 RMS deviation of F1900 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1920 RMS deviation of F1920 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1940 RMS deviation of F1940 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1960 RMS deviation of F1960 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F1980 RMS deviation of F1980 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2000 RMS deviation of F2000 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2020 RMS deviation of F2020 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2040 RMS deviation of F2040 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2060 RMS deviation of F2060 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2080 RMS deviation of F2080 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2100 RMS deviation of F2100 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2120 RMS deviation of F2120 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2140 RMS deviation of F2140 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2160 RMS deviation of F2160 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2180 RMS deviation of F2180 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2200 RMS deviation of F2200 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2220 RMS deviation of F2220 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2240 RMS deviation of F2240 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2260 RMS deviation of F2260 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2280 RMS deviation of F2280 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2300 RMS deviation of F2300 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2320 RMS deviation of F2320 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2340 RMS deviation of F2340 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2360 RMS deviation of F2360 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2380 RMS deviation of F2380 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2400 RMS deviation of F2400 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2420 RMS deviation of F2420 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2440 RMS deviation of F2440 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2460 RMS deviation of F2460 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2480 RMS deviation of F2480 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2500 RMS deviation of F2500 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2520 RMS deviation of F2520 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2540 RMS deviation of F2540 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % e_F2740 RMS deviation of F2740 number=1 RMS deviations of the observations (fields named 'e_Fnnnn') are given as a percentage: (100/<F>) * SQRT( SUM((F_i - <F>)**2)/(n-1) ) where F_i is the individual flux at wavelength lambda <F> is the average flux at wavelength lamda n is the number of averaged observations (field Spectra) % HD2 Henry Draper Catalog (HD) number (repeated) --- m_HD2 Additional HD IDs (given as '/n') --- Flamsteed Flamsteed number prefix --- VarName Variable star letter designation --- Greek Greek letter coded as alpha --- GreekSup Greek letter superscript --- m_GreekSup Second component --- Constell Constellation abbreviation --- RAh Hours RA, epoch 2000.0 h RAm Minutes RA, epoch 2000.0 min DE- Sign Dec, epoch 2000.0 --- DEd Degrees Dec, epoch 2000.0 deg DEm Minutes Dec, epoch 2000.0 arcmin SpType Spectral type --- LumClass Luminosity class information --- Vmag V magnitude in the UBV system mag VarFlag 'V' if star confirmed to be variable --- n_Vmag '*' if V from HR, HD or SAO catalogues --- B-V B-V color in the UBV system mag U-B U-B color in the UBV system mag E(B-V) B-V color excess, E(B-V) mag n_E(B-V) '*' if E(B-V) extrapolated (see adc.doc) --- RotVel Projected rotational velocity (v sin i) km/s Refs Coded reference numbers (see adc.doc) --- adc.doc ADC Documentation Francois Ochsenbein CDS 1995 Jan 03 UNKNOWN UNKNOWN * From the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory /spectro/uvbs. * An unresolved problem as reported in the ADC Electronic Newsletter Volume 2, Issue 1 (January 1993). ---------------------------------------------------------------- Ultraviolet Bright Star Spectrophotometric Catalog (SPECTRO/UVBS) Submitted by W. Landsman, Hughes STX ---------------------------------------------------------------- I have found a problem with the TD-1 bright star spectrophotometric catalog (UVBS) as it appears in the ADC CD-ROM. The problem is the loss of precision in the fluxes of the TD1 spectrophotometric catalog due to the processing done at Goddard. To quote from Section 4 of the documentation: "The flux was initially given at each of the 61 wavelengths in a E9.3 format in units of erg/(cm^2 s^1 A^1). These quantities were multiplied by 10^10 so that they could be given in a F6.2 format in units of 10^-10 erg/(cm^2 s^1 A^1), thus reducing the logical record length by 183 bytes." Unfortunately, the above process takes a flux of 5.23E-12 and transforms it to 0.05 losing two significant digits. The number of stars with fluxes less than 1e-11 is quite small, but many stars have fluxes less than 1e-10 and lose 1 significant digit in the ADC CD-ROM version of the catalog. * 03-Jan-1995: a few errors corrected for UVBS: 929 (U-B value) 1019 (misalignment of Greek letter) 1039 (E(B-V) value) 1040 (E(B-V) value) 1170 (misalignment of Greek letter) III_39A.xml A Spectral Survey of the Southern Milky Way I. General Description and Catalogue I. l = 306deg to 318deg 3040A III/40A Spectral Survey Southern Milky Way Uniform A Spectral Survey of the Southern Milky Way I. General Description and Catalogue I. l = 306deg to 318deg A Sundman L O Loden B Nordstroem Astron. Astrophys. Suppl. 16 445 1974 1974A&AS...16..445S A Spectral Survey of the Southern Milky Way I. General Description and Catalogue I. l = 306deg to 318deg B Nordstroem Astron. Astrophys. Suppl. 21 193 1975 1975A&AS...21..193N A Spectral Survey of the Southern Milky Way I. General Description and Catalogue I. l = 306deg to 318deg L O Loden K Loden B Nordstroem A Sundman Astron. Astrophys. Suppl. 23 283 1976 1976A&AS...23..283L Milky Way Surveys Spectral types The spectral survey, carried out at the Stockholm Observatory, was initiated by B. Lindblad. The observational material was obtained by L.O. Loden, K. Loden and others in the years 1956-1965, when the Stockholm Observatory took part in a joint enterprise for using the Harvard-Boyden station. The Swedish Natural Science Research Council, the Royal Academy of the Sciences, and the K. and A. Wallenberg Foundation funded the observations, which are based on both direct and objective prism plates. The data were published in three parts, the first having less precise positions than the others. The coordinates for Catalogue I (3033) were later recomputed with the same reduction procedure as Catalogues II (3034) and III (3035), making the present catalogue uniform (Andersen, 1977). The files include star identification, finding chart identification, RA and Dec, galactic longitude and latitude, spectral type, blue magnitude, visual magnitude and remarks. The data concerning the part 2 were revised by Brian Skiff in November 1996 (see the History section)
Part I Sundman+ (1974A&AS...16..445S) Part II Nordstroem (1975A&AS...21..193N) Part III Loden+ (1976A&AS...23..283L) RAh Right Ascension (1950.0) hours number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue h RAm Right Ascension (1950.0) minutes number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue min DE- Declination (1950.0) sign number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- DEd Declination (1950.0) degrees number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue deg DEm Declination (1950.0) arcminutes number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue arcmin u_DEm Uncertainty flag for coordinates number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- ID Identification (HD, HDE or DM) number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- Chart Chart number (data2 only) number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- CatNum Catalogue number (reference to finding charts) number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- m_CatNum Catalogue number suffix number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- m(B) Blue magnitude number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue mag u_m(B) Uncertainty flag for m(B) number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- Sp Spectral type Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- Rem Remarks Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- GLON Galactic longitude number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue deg GLAT Galactic latitude number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue deg Vmag Visual magnitude (data1 only) number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue mag u_Vmag Uncertainty flag for Vmag number= Spectral type, left-justified. A colon following the spectral type (not aligned) indicates an uncertain spectral type or luminosity is given in rem number= Remarks, left-justified. The following codes are used: O = overexposed U = underexposed ID = uncertain identification ST = photoelectric standard VAR(?) = Variable (possibly var.) E = emission K (?) = Interstellar K line (possibly) visible N (NN) = Diffuse (very diffuse) lines SB ? = possibly spectroscopic binary I - V = luminosity classes WD = probably white dwarf * = see special remark in printed catalogue --- Part II Revised by B. Skiff (see History) [N75] Running number number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue --- RAh Right Ascension J2000 (hours) number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue h RAm Right Ascension J2000 (minutes) number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue min RAs Right Ascension J2000 (seconds) number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue s DE- Declination J2000 (sign) number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue --- DEd Declination J2000 (degrees) number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue deg DEm Declination J2000 (minutes) number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue arcmin DEs Declination J2000 (seconds) number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue arcsec posSource Source of position the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue --- Name Identification of the star in DM and HD number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue --- Chart Chart number number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue --- Bmag Blue magnitude number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue mag u_Bmag Uncertainty flag on Bmag number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue --- SpType Spectral type number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue -- NoteFlag an additional note exists in n75_n.dat number= the position sources are: C = Carlsberg Meridian Catalogues (<I/147>, <I/170>, <I/189>, <I/205>, <I/213>) G = GSC (Guide Star Catalogue) <I/220> N = Nesterov (HDE stars, cat. <III/182>) P = PPM (catalogues <I/146>, <I/193>, <I/208>) U = USNO A0.9 catalogue --- Note Additional notes and identifications number=2 Nordstrom comment codes are: D = overlapped spectrum K = interstellar K line visible U = underexposed O = overexposed --- Notes to n75.dat [N75] Running number as in n75.dat --- Cont Continuation symbol --- Text Text of note --- Francois Ochsenbein CDS Brian Skiff Lowell Obs. 1996 Nov 26 Thanks are due to Dr Johannes Andersen, who provided the data on magnetic tape to Dr Carlos Jaschek (CDS) as early as January 1977. The first version of this description file was done by Julie Anne Watko [SSDOO/ADC] in August 1996. UNKNOWN UNKNOWN * November 1996: addition of the file n75.dat, a revision of data2.dat, was prepared by Brian Skiff <bas@lowell.edu>. The positions, magnitudes, cross-identifications and notes have been improved as follows: - the GSC (Guide Star Catalogue version 1.1) was used to derive a position, by a comparison with the published charts; a few problem cases were checked against the digitized sky survey; positions were then improved with the PPM catalogues (<I/193> and <I/208>) - SIMBAD was searched around each position for cross-identifications (resulting also in SIMBAD fixes). The printed versions from Goddard of Durchmusterungen CoD <I/114> and CPD <I/108> were then searched for additional IDs by comparing positions and charts. - the Mermilliod's Lausanne photometric database was used to improve the B magnitudes. - the comments have been added. III_40A.xml Catalogue of selected spectral types in the MK system 3042 III/42 Selected MK Spectral Types Catalogue of selected spectral types in the MK system M Jaschek Bull. Inform. CDS 15 121 1978 1978BICDS..15..121J MK spectral classification Spectral types The catalog provides a single spectral type for each star listed in the La Plata catalog (Jaschek, Conde and de Sierra 1964; catalog <III/18>) and in the MK Extension (Kennedy 1978; see catalog <III/78>). In all cases the classifications are selected from those in the literature and have not been made by the author specifically for this compilation. A selected classification is considered to be the best one but is not necessarily a good one. If only one classification exists for a given object, it is given, regardless of its quality. The classifications were selected using a weighting system, with highest weight being given to classifications made by Morgan and/or Keenan, somewhat lower weight to those made by other spectral classification experts and various lower weights to those made by other workers. Classifications using designations that do not appear in the MK system have been excluded, as have objective-prism classifications, except where no slit spectra were available. The catalog contains a running number in one of the original catalogs (sequential numbers in the machine versions), identification of the original catalog, star identification (HD, DM, miscellaneous designations), equatorial coordinates (B1900), magnitude, V if available, m(v) otherwise) for reference purposes, reference number in the original catalog, selected classification, dispersion information, and standardized reference.
The catalog of Selected MK Types Number Running number in one of the original catalogues --- cat Original catalogue: J or K (J) La Plata Catalog of Stellar Spectra Classified in the MK System, by Jaschek et al. (1964, catalog <III/18>) (K) MK Classification Extension by Kennedy P.M. (kept up-to-date; latest version available is <III/78>) --- Name Identification of the star (generally HD or DM number) --- RAh Right Ascension 1900 (hours) h RAm Right Ascension 1900 (minutes) min DE- Declination 1900 (sign) --- DEd Declination 1900 (degrees) deg DEm Declination 1900 (minutes) arcmin Vmag V magnitude The value 99.99 = nebular? (Star #3542) mag n_Vmag 'V' for variability --- MK Source and number of available MK types --- Ref Reference number in the original catalogue --- SpType Selected spectral classification --- Disp Dispersion used (in Angstroem/mm) for the selected classification the dispersion is followed by abbreviations for the dispersive system used: OP = Objective Prism ; P = Prism ; G = Grating 10-7 RefCode Bibliographical coded Number, used for the BSI (Spite et al., 1980) --- BibCode Standardized bibliographical code --- The References RefCode Bibliographical Reference Code (repeated if several lines) --- Text Text of Reference --- Julie Anne Watko SSDOO/ADC Francois Ochsenbein CDS 1996 May 11 UNKNOWN UNKNOWN The original version contained vertical bars as separators, and a few control characters. There were removed at ADC, and the standardized BibCode, as used by SIMBAD, was added at CDS. III_42.xml Catalogue of Luminous Stars in the Southern Milky Way 3043 III/43 Luminous Stars in the Southern Milky Way Catalogue of Luminous Stars in the Southern Milky Way C B Stephenson N Sanduleak Publ. Warner & Swasey Obs. 1 ??? ??? 1971 1971PW&SO...1....1S III/76 : Luminous Stars in the Northern Milky Way. J/ApJS/97/189 : A Spectroscopic Database for LSS stars by Reed and Beatty Milky Way Stars, luminous Spectral types This Catalogue represents an extension to the entire Southern Milky Way of the objective-prism survey for intrinsically luminous stars in the Northern Milky Way <III/76> that was carried out jointly by the Hamburg and Warner and Swasey observatories. The object has been to survey the Southern Milky Way with plates as similar as possible to the plates used for the Northern Milky Way, including similarity of limiting magnitude. To this end the objective prism that was used with the Warner and Swasey Schmidt telescope for the Northern survey was sent to Cerro Tololo, Chile, where it was used by Sanduleak to photograph the Southern Milky Way with the Schmidt telescope of the University of Michigan. The survey was planned to have a minimum extent in galactic latitude of +/-10deg. On each field three spectral plates were taken, all intended to have spectral widening near 0.2 mm. One blue-region (Kodak IIa-O) plate was given an exposure of 11 minutes, and another was double-exposed for 3 minutes and 10 seconds. A red plate (Kodak 103a-F plus Schott GG 14 filter) was also taken for the detection of any appreciable Halpha emission, with three exposures nominally 9 minutes, 1 minute and 10 seconds. The dispersion is 580 Angstroems/mm at Hgamma and about 1000 Angstroems/mm near Hlpha; a Michigan objective prism of 4deg angle, was used to obtain the Halpha plates. The spectral classification system is that discussed by Slettebak and Stock (1957) and Nassau and Stephenson (1960). An important result of the generally excellent quality of the new survey plates is that the ce stars (OB stars apparently having the Balmer continuum in emission) are easily recognised. The magnitudes are based upon eye estimates of image density on the blue-region spectral plates, calibrated by published magnitude sequences, and are generally characterised by a probable error of 1/3 to 1/4 mag. The equatorial coordinates for the stars have been derived from measurements of the objective-prism plates, using the SAO <I/131> catalogue for reference stars. The positions derived in this way are accurate to 1" to 2" of arc, providing spectral lines are visible for measurement. When spectral lines are not visible, the coordinate parallel to the spectral dispersion -- always the declination -- becomes 10" or somewhat more uncertain.
The LSS Catalogue Mod Not blank if modifications have been done to the original catalogue --- LSS Designation in the catalogue --- DM Durchmusterung (BD north of -22deg, or CD) identification from the original catalogue --- n_DM Note (North, South, Following, Preceding) about DM identification --- SpType Spectral type from original catalogue number=1 spectral annotations (all reported in uppercase letters): ce means that the Balmer continuum appears to be in emission; le means that at least one emission line, nearly always a Balmer line, is visible on a blue region plate; h means that Halpha was noted in emission on an independently scanned Halpha plate; r means that the spectrum appears distinctly reddened; rr means that the spectrum appears extremely reddened. : a colon means that everything preceding it is uncertain, () parentheses means that the data within the parentheses are uncertain; ! an exclamation point denotes that the datum immediately preceding it is exceptionally pronounced. Ia+ A luminosity class of Ia+ indicates an apparent luminosity brighter than Ia. * Newer classifications by Reed and Beatty, 1995 =1995ApJS...97..189R --- Pmag Photographic magnitude 0.1mag u_Pmag Uncertainty flag (:) on Pmag --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAds Right Ascension 1950 (deci-seconds) 0.1s u_RAds Uncertainty flag (:) on RA --- DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec u_DEs Uncertainty flag (:) on DE --- Rem Remarks number=2 the remarks include: - Previously published spectral type given in the catalogue of Jaschek et al (1964) for HD stars; - designation in the 2d edition of the General Catalogue of Variable Stars for stars for which a DM number is given; - presence in the Catatogue of Stars Suspected of Variability (indicated by "CSV"), for stars with a DM number; - designation in the Innes double-star catalogue (SDS) or that of Aitken (ADS), for stars with a DM number; - designation in the Bright Star Catalogue. - the notation "Hbeta wk" means that the Balmer decrement (not merely Hbeta) is abnormal, suggesting that there is unseen line emission in the blue region. - the remark that the ultraviolet is steep or weak usually means that there is a suspicion of a Balmer jump. - "Flat continuum" refers to an OB star that is unusually intense in the ultraviolet and exceptionally lacking in apparent space reddening; such stars are sometimes white dwarfs, hot subdwarfs, old novae, etc. - "R" indicates further remarks in the notes (file "rem") to the catalogue; these notes often contain information relevant to identifying a star in a crowded region. --- DM1 DM identification from CSI number=3 designations from the Catalogue of Stellar Identifications (CSI developed at CDS) are indicated .. as the first two letters; the other designations in the first two letters are BD (Bonn), CD (Cordoba), or CP (Cape Photographic) --- DM2 Second DM identification number=3 designations from the Catalogue of Stellar Identifications (CSI developed at CDS) are indicated .. as the first two letters; the other designations in the first two letters are BD (Bonn), CD (Cordoba), or CP (Cape Photographic) --- HD Henry Draper Catalogue identification --- Remarks and Notes LSS Designation in the catalogue --- Text Text of remarks; LSS is repeated when the text is made of several lines --- Francois Ochsenbein CDS 1995 Oct 05 UNKNOWN UNKNOWN * Errors in the "Luminous Stars in the Milky Way" reported by Bischoff M. =1978BICDS..14...15B * Version 25-Oct-1993: First electronic description. * Version 14-Apr-1994: HD number of LSS 1969 reported by S. Nishimura changed from 30562G to 305627 * 05-Oct-1995: Standardized the Documentation at CDS, and added the Description and Notes in this file. References: Jaschek, C., Conde, H., and Sierra, A.C., 1964, Obs. Astron., La Plata, Serie Astronomica, XXVIII (2). Nassau, J.J., and Stephenson, C.B, 1960, Astrophys. J., 132, 131. Slettebak, A,, and Stock, J. 1957, Zeitschr. Astroph., 42, 67. III_43.xml An Atlas of Stellar Spectra 3044 III/44 Atlas of Stellar Spectra An Atlas of Stellar Spectra H L Johnson Rev. Mex. Astron. Astrof. 2 71 1977 1977RMxAA...2...71J An Atlas of Stellar Spectra H L Johnson Rev. Mex. Astron. Astrof. 4 3 1978 1978RMxAA...4....3J Spectrophotometry There are exactly 8192 spectral elements (points) in each spectrum, regularly spaced in terms of frequency. The first point corresponds to spectral frequency 0, while point number 8193 (not included) corresponds to the laser frequency. The 632.8nm laser frequency was doubled, producing an effective laser wavelength of about 316.4nm. Tentatively, it may be assumed that the exact laser wavelength is 316.43nm. The spectra have been normalized so that the bluest stars are approximately level from 480 to 1000nm. The spectra are linear in intensity with zero intensity at tabulated zero. It was not possible to make satisfactory atmospheric extinction corrections throughout all of the atmospheric bands; at places where corrections could not be made, the spectra were set (exactly) to zero. Some of these spectra have been published already (H.L. Johnson, Rev. Mex. Astron. Astrof. 2, 71, 1977); the remainder will be published soon (Rev. Mex. Astron. Astrofis., 4, 3). These published spectral plots contain in graphical form the information needed to evaluate the signal-to-noise ratios of the spectra on this tape. (From Harold L. Johnson, Dec. 13, 1977)
The Atlas Name Name of the star --- I 8 Spectral elements (pixels); there are 1024 lines per star. There are therefore 8192 points per spectrum. number=1 with the values assumed in the Description, the values of the wavenumbers, expressed in cm-1, are given by SIGMA(I) = 3.8577 * (I-1) and wavelength, in Angstroems, by WAVELEN(I) = 1.E8/(3.8577 * (I-1)) --- starlst.txt List of the stars Melissa C. Larkin SSDOO/ADC 1997 May 05 The original "Intro" was prepared by CDS and used to create this ReadMe file. III_44.xml Infrared Spectra for 32 Stars 3045 III/45 Infrared Spectra for 32 Stars Infrared Spectra for 32 Stars H J Johnson M E Mendez Astron. J. 75 785 1970 1970AJ.....75..785J Spectra, infrared Relative fluxes are presented for 44 spectra of 32 stars, ranging in spectral type from A0 to M7. Spectra of seven carbon stars are included. Although some spectra cover the wavenumbers from 2500 to 8200, many spectra do not include wavenumbers less than 4000 and there are many gaps as a result of atmospheric absorption.
Spectrum of Alpha Lyrae Spectrum of Alpha+Canis Majoris Spectrum of Alpha Canis Majoris Spectrum of Moon (sun) Spectrum of Alpha Bootis Spectrum of Gamma Draconis Spectrum of Alpha Tauri Spectrum of Alpha Tauri Spectrum of Delta Ophiuchi Spectrum of Beta Pegasi Spectrum of Beta Pegasi Spectrum of Eta Geminorum Spectrum of Mu Geminorum Spectrum of Rh Persei Spectrum of R Lyrae+ Spectrum of R Lyrae Spectrum of R Lyrae Spectrum of Eu Delphini Spectrum of Omicron Ceti Spectrum of Omicron Ceti Spectrum of R Hydrae Spectrum of R Cassiopeiae Spectrum of R Leonis Spectrum of Chi Cygni Spectrum of Alpha Orionis Spectrum of Alpha Orionis Spectrum of Alpha Scorpii Spectrum of Mu Cephei Spectrum of Mu Cephei Spectrum of Mu Cephei Spectrum of Delta 2 Lyrae Spectrum of Alpha Herculis Spectrum of Alpha Herculis Spectrum of VY Canis Majoris Spectrum of UU Aurigae Spectrum of W Orionis Spectrum of Y Canum Vanaticorum Spectrum of X Cancri Spectrum of 19 Piscium Spectrum of T Lyrae Spectrum of T Lyrae Spectrum of U Hydrae Spectrum of Venus/moon 3-3 Spectrum of Jupiter/moon 4-22 wavel Wavelength in Angstroem nm flux relative flux in line --- N.P.M. Kuin and Nancy G. Roman ADC 1995 Oct 24 UNKNOWN UNKNOWN The author provided originally neither wavenumbers nor flux units. The wavenumber corresponding to a given flux value could be obtained approximately from the formula: Wavenumber = 4.5*(10*linenumber + ending digit of lable) - 37 (For the ending digit of lable the index of the value in the record has been used, starting with zero. There were 10 values per record.) It was important to use the line number that was given in a column following the data values, since many lines with no flux values have been deleted at the beginnings and ends of each file. UNKNOWN UNKNOWN Detailed description of files: ----------------------------------------------------------------------------- 1 Alpha Lyrae A0 V 3900-8200 2 Alpha+Canis Majoris A1 V March 3, 1969 2400-8200 3 Alpha Canis Majoris A1 V Sum 2400-8200 4 Moon (sun) G2 V May, 1968 3900-8200 5 Alpha Bootis K2 III p March 14, 1968 3900-8200 6 Gamma Draconis K5 III May 18,1968 3900-8200 7 Alpha Tauri K5 III March 14,1968 3900-8200 8 Alpha Tauri K5 III Mean 2400-8200 9 Delta Ophiuchi M0.5 III March 23, 1968 3900-8200 10 Beta Pegasi M2-3 II-III+ September 1,1968 2400-8200 11 Beta Pegasi M2-3 II-III Mean 2400-8200 12 Eta Geminorum M3 III February 20, 1968 3900-8200 13 Mu Geminorum M3 III Mean 2400-8200 14 Rh Persei M3 II III December 5,1968 2400-8200 15 R Lyrae+ M5 III May 27, 1968 3900-8200 16 R Lyrae M5 III September 5,1968 2400-8200 17 R Lyrae M5 III Mean(Sept 5,6, 1968) 2400-8200 18 Eu Delphini M6 III Mean(Apr 5,6, 1968) 2400-8200 19 Omicron Ceti M6 e 3900-8200 20 Omicron ceti M6 e 2400-8200 21 R Hydrae M7 e Mean(Spring,1968) 3900-8200 22 R Cassiopeiae M7 e September 20,1968 2400-8200 23 R Leonis M8 e February 4, 1968 3900-8200 24 Chi Cygni M p,e, s May 21, 1968 3900-8200 25 Alpha Orionis M1-2 IAB March 14, 1968 3900-8200 26 Alpha Orionis M1-2 IAB Composite 2400-8200 27 Alpha Scorpii M2 Ia 3900-8200 28 Mu Cephei M2 Ia Sum 3900-8200 29 Mu Cephei M2 Ia Mean Sept 5,6, 1968) 2400-8200 30 Mu Cephei M2 Ia August 24, 1968 2400-8200 31 Delta 2 Lyrae M4 II May 31, 1968 3900-8200 32 Alpha Herculis M5 IB-II 3900-8200 33 Alpha Herculis M5 IB-II September 1, 1968 2400-8200 34 VY Canis Majoris C M3-5 e Ia-Iab Mean 2400-8200 35 UU Aurigae C 5,3 Sum(Mar 23,25, 1968) 3900-8200 36 W Orionis C 5,3 Mean 2400-8200 37 Y Canum Venaticorum C 5,4 May 16, 1968 3900-8200 38 X Cancri C 5,4 December 6, 1968 2400-8200 39 19 Piscium C 6,2 Mean 2400-8200 40 T Lyrae C 6,5 Mean(8/24,+9/1,1968) 2400-8200 41 T Lyrae C 6,5 August 24, 1968 2400-8200 42 U Hydrae C 7,3 February 20, 1968 3900-8200 43 Venus/moon 3-3 March 3, 1969 2400-8200 44 Jupiter/moon 4-22 April 22, 1968 3900-8200 45 Jupiter/moon 4-22 April 19, 1968 3900-8200 III_45.xml Catalogue of Ap and Am Stars 3046 III/46 Ap and Am Stars Catalogue of Ap and Am Stars Ch Bertaud M Floquet Astron. Astrophys. Suppl. 16 71 1974 1974A&AS...16...71B Catalogue of Ap and Am Stars W P Bidelman D J MacConnell Astron. J. 78 687 1973 1973AJ.....78..687B Stars, Am Stars, Ap Stars, peculiar This catalogue contains identifications of stars with peculiar spectra (Ap) and metallic lines (Am). Identifications are HD or HDE, or alternatively a DM number.
Am Stars Ap Stars M/P Peculiar or Metallic --- DM Durchmusterung zone and number Field is left justified with one space between zone and number. Zone always includes sign, but does not include preceding zeros for single-digits. --- HD Henry Draper number or HD Extension number --- Julie Anne Watko SSDOO/ADC 1996 Jul 15 III_46.xml Catalogue of Stellar Radial Velocities 3047B III/47B Stellar Radial Velocities 0-20 hrs Catalogue of Stellar Radial Velocities D S Evans IAU Symp. 30 57 1967 1967IAUS...30...57E Radial velocities The Interim Supplement to the General Catalogue of Stellar Radial Velocities (Evans 1979, ISGCRV) contains radial velocities for stars with right ascensions from O through 20 hours. The ISGCRV is intended as a continuation of the General Catalogue of Stellar Radial Velocities (Wilson 1953, GCRV). The ISGCRV resulted from a literature search and data reduction by D. S. Evans covering approximately the years 1951-1977. It contains adopted velocities on the Mount Wilson system. Unfortunately, the individual mea- surements and the literature references could not be included in this version. Both for this reason, and because the ISGCRV covers only O through 20 hours of right ascension (equinox 1900), the ISGCRV should be used with the Bibliography of Stellar Radial Velocities (Abt and Biggs 1972), or the Bibliographical Star Index Retrieval System (Hill et al. 1984).
Catalog Data ID Star id Name of star (Henry Draper number when available). Some H II regions and planetary nebulae are also included. --- RAh Right ascension, equinox 1900 (hours) h RAm RA minutes min RAflag RA approx flag Colon (:) signifying approximation --- DE- Dec sign --- DEd Declination, equinox 1900 (degrees) deg DEm Dec arcminutes arcmin DEflag Dec approx flag --- ComA Note on magnitudes A letter signifying a component of a multiple system, a left parenthesis, (, for non-photoelectric visual magnitudes, or an asterisk (*) for Henry Draper magnitudes. This comment applies to magnitude 1. --- Mag1 Magnitude (V) 1 For one star, HD 16157, this value is given as var? in the proof copy; in this version, 99.99 is used instead. mag ComB Second note on magnitudes Letters signifying components of multiple system, the letter V (unknown meaning), colon (:) for approximate, or plus (+) for greater than. The colon and plus apply to magnitude 1, and the other notations apply to magnitude 2. --- Mag2 Magnitude (V) 2 Implies a multiple system. The comment fields specify the components. mag n_Mag3 Component to which Mag3 applies --- Mag3 Magnitude (V) 3 Implies a multiple system. The comment fields specify the components. mag Spect Spectrum Given in the customary form. The main spectral type is always in byte 58, leaving room in bytes 56-57 for Mount Wilson luminosity classes, such as sd and c. An asterisk (*) in byte 58 signifies an H II region or planetary nebula, according to the notation accompanying it. --- Vel Velocity km/s VelCom Vel comment Colon (:) for approximation; or right parenthesis ")" for parentheses in the proof copy, which appear to indicate a question about the identity or type of the object to which the velocity applies. In one case, HD 196877, this byte contains a 9, which is the hundredths' digit of the velocity. This field can also be blank. --- Quality Quality A rating from A through E, in the system of the GCRV. The rating itself will always be in byte 87, if given. Byte 88 can contain a question mark (?) or blank. A number of velocities were not assigned a quality rating. --- Pcnt Plate count Total number of plates measured for all the velocities used to arrive at the adopted velocity. --- PcntCom P count comment Comment on plate count. Can be a question mark (?), a plus (+) meaning greater than, or blank. --- ObsCode Observe Code Abbreviations for observatories (or observers), separated by commas. --- GCRVnum GCRV number Catalog number given for the star by Wilson (1953) --- flag1 Var vel flag Var vel flag. Letter V for variable velocity, or else blank. --- flag2 Var mag flag Var mag flag. Letter M for known variable, or else blank. --- flag3 Multiple flag Multiple flag. Letter D for double or multiple star, or else blank. --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 22 UNKNOWN UNKNOWN Other versions of the ISGCRV have been distributed, but this one supersedes them, as it was corrected from a set of proof copies supplied by Evans, which included corrections and additions by several referees. Xeroxes of Evans's data file containing the results of the literature search were also available to us. UNKNOWN UNKNOWN The Astronomical Data Center (ADC), NASA Goddard Space Flight Center, received the Interim Supplement to the General Catalogue of Stellar Radial Velocities on magnetic tape from the Centre de Donnees Stellaires, Strasbourg, France, in 1981. That version contained 80-byte card images. Different parts of the catalog had been keypunched at different sites, so that there was variation not only in the format, but also in the kinds of data fields included. For example, some sections included catalog numbers from the GCRV, and some did not. Also, an attempt had been made to code spectra in a condensed format, but consistency and completeness were not achieved. The modifications to this version comprised several steps: 1. The three parts of the catalog were merged in a uniform format. A sequential number was assigned to each record. For clarity, different kinds of names were temporarily assigned to different fields. 2. The resulting file was proofread against the proof copies from Evans. At this stage, it turned out that not all the proof copies were identical. Evans had sent some of them to various radial velocity specialists for review. Some of the keypunching in France was done from the resulting revised version, and some was not. 3. The corrections, coded by the proofreader on 80-column forms, were themselves keypunched and proofread. 4. Now it was necessary to adopt a consistent policy on the revisions made by referees. It was decided to incorporate new photometry without comment, since these data are not primary. Velocities from the referees have also been included, but are listed in Figure 3 on page 8. The proofreader's corrections were amended in accordance with this policy, after a re-examination of all the proof copies. 5. A Fortran program was used to apply the amended list of proofreader's corrections to the catalog. 6. A Snobol program was used to convert the spectra to a conventional format. This program was partly interactive, in that it required real-time intervention either to confirm the program's modification, or to supply a substitute for that modification. The catalog was split into eight parts for this program. The output files were then merged again. 7. During the preceding steps, a list of special problems had been maintained. These difficulties were now resolved. Several corrections were made with an interactive text editor, and a number of omitted records were inserted in the same way. 8. Again by means of a text editor, GCRV numbers (previously given in only part of the machine-readable version) were added. 9. Many records in the machine-readable version as received had asterisks that seemed in most cases to denote double stars. The source of this information was the proof copies of the ISGCRV notes from Evans (not part of the current catalog). But these notes seemed to have been misinterpreted so frequently by the original keypunchers that in several parts of the catalog, the asterisk meant, in practice, no more than unusual star. The notes were re-examined, and the flags in bytes 111-113 were substituted for the asterisks. 10. Blank fields and sequential line numbers were deleted, and the name fields were merged. The present 114-byte record resulted. 11. An ADC utility program was run to check for invalid numerical values. A few corrections were made with a text editor. The known referees consulted by Evans on this catalog are the following: D. Crampton, J. Elliott, C. Fehrenbach, W. Gliese. It is not certain that this list is complete. The source for these names is the notations on the proof copies that were available to us. The referee who gave each individual velocity in Figure 3 (below) had to be guessed from handwriting. Every name in that list is uncertain to some extent. Moreover, it is evident that none of the referees reviewed the entire catalog. In any case, the referees should not be held responsible for any of the catalog's contents, although we acknowledge their work and hope that we have made good use of it. The adopted velocities, except for the few listed in Figure 3(below), are due entirely to Evans. The responsibility of the authors of this document is limited to transcription and, sometimes, interpretation. We made no effort to evaluate or amend the adopted velocities--only to produce a good machine-readable version of the results as they were available to us. We lament our inability to produce a good scientific introduction to the ISGCRV, but such an endeavor would have exceeded both our time and our expertise. Figure 3. Referees' Velocities Star R.A. Referee (see text) HD 236672 01 08.4 Crampton? HD 8492 01 18.9 Gliese? HD 8570 01 19.6 Gliese? HD 8642 01 20.2 Gliese? HD 8736 01 21.1 Gliese? HD 9518 01 28.4 Gliese? BD +62 282 01 31.1 Gliese? HD 10285 01 35.5 Gliese? -------- 01 35.5 Gliese? BD +60 317 01 36.8 Gliese? HD 12302 01 55.6 Crampton? HD 129S3 02 01.7 Crampton? HD 13267 02 04.6 Crampton? HD 237007 02 42.7 Crampton? HD 23243 03 38.5 Gliese? HD 23478 03 40.4 Crampton? HD 23565 03 41.1 Gliese? HD 232843 03 41.3 Gliese? HD 23860 03 43.3 Gliese? HD 232848 03 43.8 Gliese? HD 232850 03 45.0 Gliese? HD 232861 03 49.9 Gliese? BD +Sl 816 03 51.4 Gliese? HD 25215 03 55.2 Gliese? HD 33152 05 03.2 Crampton? HD 34921 05 15.8 Crampton? HD 37318 05 32.6 Crampton? HD 42690 06 07.0 Elliott?? HD 44738 06 18.3 Elliott?? HD 46860 06 30.5 Elliott?? HD 68397 08 07.0 Elliott?? HD 74678 08 40.2 Elliott?? HD 97503 11 08.0 Gliese HD 102392 11 41.9 Gliese? HD 110315 12 36.1 Gliese HD 111417 12 44.0 Gliese HD 113827 13 01.3 Gliese BD +50 2030 13 48.1 Gliese HD 126053 14 18.1 Gliese BD +24 2733B 14 21.0 Gliese HD 129002 14 35.1 ?? BD +27 2411 14 39.0 Gliese HD 1329S0 14 56.9 Gliese HD 148467 16 23.2 Gliese HD l51995 16 45.7 Gliese ADC update July 1995: The documentation was converted to standard form. During verification some errors were found. The following 2 changes should be noted: In record 4098 the Mag1 value was changed from "10. 0" to "10.09". In record 6814 the plate count value was aligned "4 " to " 4". The original records could not be consulted for these changes. III_47B.xml Spectrophotometric Scans 3048B III/48B Spectrophotometric Scans Spectrophotometric Scans M Breger ApJS 32 7 1976 1976ApJS...32....7B Spectrophotometry This data set contains 937 sets of spectrophotometric observations of stellar continuua made in the 3200-12000A region. The data were transformed to the Hayes and Latham (1975) calibration of Alpha Lyrae. Bandpasses vary between 10 and 100A. An analysis of the errors in the catalog appears in Breger (1976). Note that scans of the southern stars observed by Gutierrez-Moreno et al. (1968) are NOT corrected for the right ascension effects discussed in Breger (1976).
Catalog Data StarName Star name --- Cat Catalogue number, usually a Harvard Revised (HR) = Yale Bright Star (YBS) or Henry Draper (HD) number. --- B-V (B-V) color (B-V) color taken from the Blanko et al. (1970) UBV Catalogue, the Bright Star Catalogue or the original spectrophotometric source. --- Sp Spectral type as taken from the same sources as the B-V color. --- BW Bandpass width used; sometimes two bandpass widths are given and are separated by a slash ( / ) 0.1nm Obscode Observer code - (right justified). --- Num The number(N) of wavelength (0.1nm)- magnitude pairs given. If this is less than the maximum value of 35 the remainder of each logical record is filled with zeroes. --- WaveLen Wavelength 0.1nm Mag Magnitude The magnitude refers to the conventional magnitude per unit frequency. mag C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 22 UNKNOWN UNKNOWN The Catalog of Spectrophotometric Scans of Stars (Breger, M. 1976, Ap.J. Supp., 32, 7.) was received in machine-readable form from Dr. S. Parsons (University of Texas) on March 11, 1976. The version as received consisted of a 7-track 800 bpi magnetic tape with two files. The first file contained the analysis program as written for the CDC 6600 computer and the second file represents the original data. The analysis program was then converted to run on the IBM S/360 at NASA/GSFC and the data was processed. Some corrections to the original analysis program had to be made due to the differences in the computers, but since the result of the analysis was a listing of the data as given in the above reference - checks were possible at every step of the analysis. The output was then reformatted so that the data would be in a format that allowed easy access to the data. As the catalogue was checked out, a number of star name errata were noticed. A list of Corrected errata in catalogue HR Number Page Published Fixed machine- Name Number Catalogue readable record HR 718 14 X12 CET XI2 CET HR 984 17 EPSILON ERI ZETA ERI HR 5843 58 XI SER CHI SER HR 6493 63 55 XI SER blank KAPPA VEL 40 HR 3731 HR 3734 HR 3659 39 ALPHA CAR a CAR HR 8937 85 BETA SCI BETA SCL HR 8937 85 BETA SCI BETA SCL DELTA ORI 27 HR 1851-2 HR 1851 XI SCO 59 HR 5977/8 HR 5977 Note: A lower case a was used for star HR 3659 (a CAR) -------------------------------------------------------------------------------- III_48B.xml White Dwarfs 3049 III/49 White Dwarfs, Selected Data White Dwarfs W J Luyten Univ. of Minnesota Press ??? ??? 1970 1970 Stars, white dwarf X-ray sources This is a selected set of data from the Luyten White Dwarf Catalogue (Luyten 1970) as extracted by Dr. G. Share of the Naval Research Laboratory. Each record in the catalog contains the name of the celestial source, an equatorial position, an X-ray intensity, and comments.
Catalog Data Name Name of celestial source --- RAd Right Ascension 1950.0 (unit=degrees) deg DEd Declination 1950.0 (unit = degrees) deg XInt X-ray intensity (where applicable in units of given detector) --- rem Comments --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 22 UNKNOWN UNKNOWN The Luyten White Dwarfs Catalogue (W. J. Luyten, White Dwarfs, 1970, University of Minnesota Press) has been made machine-readable by Dr. G. Share (Naval Research Laboratory). The information given in this document has been obtained via private communication with Dr. Share. No effort has been ex- pended to verify the contents and Dr. Share bears the responsibility for any keypunching errors. III_49.xml Michigan Catalogue of two dimensional spectral types for the HD stars (Vol.2: -52 to -40 degrees) 3051B III/51B Michigan Catalogue of HD stars,Vol.2 Michigan Catalogue of two dimensional spectral types for the HD stars (Vol.2: -52 to -40 degrees) N Houk Dept. of Astronomy, Univ. of Michigan Ann Arbor, Michigan ??? ??? 1978 1978MSS...C02....0H III/31B : Volume 1 of this catalog (additional declination zones) III/80 : Volume 3 of this catalog (additional declination zones) III/133 : Volume 4 of this catalog (additional declination zones) MK spectral classification Plate data Spectral types This volume of the catalog contains all HD stars between -53.0 deg. and -40.0 deg. in B1900 declination, and is part of a series of catalogs in the University of Michigan program of systematic reclassification in the MK system of the entire Henry Draper Catalogue (HD). The stars were classified visually on objective-prism plates taken with the Michigan Curtis-Schmidt telescope at Cerro Tololo Inter-American Observatory. The 4-degree + 6-degree prisms yield a dispersion at H-gamma of 108 angstroms/mm, with a resolution of about 2 angstroms/mm, comparable to that of the original MK system. The spectra were taken on IIaO plates and widened to 0.8 mm, with 20-, 4-, and 1-min. exposures being obtained. The catalog BD includes spectral classifications, photographic magnitudes, right ascension and declination (B1900), centennial precessions, galactic coordinates, and cross identifications to the numbering systems of the HD, CD, and CPD catalogs.
The Catalogue, Vol.2 HD Henry Draper Catalog (HD) number --- Case '*' = sp. type lower case in printed ver. --- n_SpType '+' if spectral type is from HD Catalog --- SpType Spectral type --- Ave_Flag 'A' if classification used is an average. --- q_SpType Quality of the classification, see adc.doc --- Remark Remark (see adc.doc Table 5 for description) --- Ptg Photographic magnitude from HD catalog (99.99 indicates unavailable Ptg). mag Var_Flag 'V' if star is known or suspected variable --- RAh Hours RA, epoch 1900.0 h RAm Minutes RA, epoch 1900.0 min RAs Seconds RA, epoch 1900.0 s FlagPos the '*' indicates a position known to an arc-minute --- DE- Sign Dec, epoch 1900.0 --- DEd Degrees Dec, epoch 1900.0 deg DEm Minutes Dec, epoch 1900.0 arcmin DEs Seconds Dec, epoch 1900.0 (blank if FlagPos is flagged with '*') arcsec precRAm Centennial precession in RA, minutes 0.01min/yr precRAs Centennial precession in RA, seconds 0.01s/yr FlagPrec if precession in RA given to 0.1 minutes/century in the published catalog. --- precDE- Centennial precession in Dec, sign 0.01arcmin/yr precDEm Centennial precession in Dec, minutes 0.01arcmin/yr precDEs Centennial precession in Dec, seconds 0.01arcsec/yr GLON Galactic longitude deg GLAT Galactic latitude deg CPD Cape Photographic Durchmusterung identification (CP-ZZNNNNN) --- CD Cordoba Durchmusterung identification (CD-ZZNNNNN) --- Plate1 Plate code #1 (see file plates.dat) --- Plate2 Plate code #2 (see file plates.dat) --- Plate3 Plate code #3 (see file plates.dat) --- Plate4 Plate code #4 (see file plates.dat) --- Remarks of Vol.2 HD Henry Draper Catalog (HD) number --- Remark Remarks in free form text --- List of Plate Codes Code Plate code --- Number Plate Number --- Date Exposure date --- adc.doc ADC Documentation Francois Ochsenbein CDS 1993 Nov 17 UNKNOWN UNKNOWN * 17-Nov-1993: list of plates added at CDS * 08-Dec-1994: list of plates corrected by Shiro Nishimura [ADAC/NAOJ] III_51B.xml Catalog of Stars Classified from the Ultraviolet Line Features of the S2/68 Experiment 3053 III/53 Stars Classified from S2/68 UV Line Features Catalog of Stars Classified from the Ultraviolet Line Features of the S2/68 Experiment A Cucchiaro M Jaschek C Jaschek CDS Inf. Bull. No. 17 93 1979 1979BICDS..17...94C MK spectral classification Spectroscopy Spectra, ultraviolet This catalog provides the spectral classifications of 1900 stars from the papers listed in References. The classifications were made from spectra obtained by the S2/68 sky survey telescope experiment aboard the TD1 satellite.
TD 1A
MK and UV spectral classification data HDpre Prefix to HD number --- HD HD number --- HR HR (Bright Stars) designation --- RAh Right Ascension (1950) hours h RAm Right Ascension (1950) minutes min RAs Right Ascension (1950) seconds s DE- Declination (1950) sign --- DEd Declination (1950) degrees deg DEm Declination (1950) arcminutes arcmin DEs Declination (1950) arcseconds arcsec V Apparent V magnitude mag SpMK MK spectral type --- SpUV UV spectral classification. --- Julie Anne Watko SSDOO/ADC 1996 Jul 15 III_53.xml Radial Velocities in Open Clusters 3055 III/55 Radial Velocities in Open Clusters Radial Velocities in Open Clusters J -C Mermilliod Bull. Inform. CDS 16 2 1979 1979BICDS..16....2M Clusters, open Radial velocities This compilation contains more than 5700 individual radial velocities for 370 stars in 4 open clusters.
The compilation LID Designation in Lausanne/Geneva system number=1 the system is described by Mermilliod (1978). The first 6 digits designate the cluster as: +2.2632 = Praesepe (M44); numbering by Klein-Wassink W.J. 1927, Publ.Kapteyn Astr.Lab. 41 Vanderlinden H.L. 1933, Etude de l'amas de Praesepe. +5.2020 = Alpha Persei cluster; numbering by Heckmann O., et al. 1956, Mitt. Hamburger Sternw. Bergedorf no 101 +5.2022 = Pleiades Hertzsprung E. 1947, Ann. Sterrew. Leiden 19,3 +5.2025 = Hyades; numbering by van Bueren H.G. 1952, Bull. Astr. Inst. Netherl. 11,385 van Altena W.F. 1966, Astron. J. 1966, 71,482 (no Va+1000) +5.2111 = Coma Berenices; numbering by Trumpler R.J. 1938, Lick Obs.Bull. 18,167 --- JD Date of observation d RV Radial Velocity km/s e_RV Probable error on RV km/s Nlines Number of lines measured --- Disp Dispersion used (Angstroem/mm) 10-7 Method Technique used: PE = photoelectric, OP = Objective prism --- Ref Reference number=2 the five first letters indicate the journal: AA = Astronomy and Astrophysics AJ = Astronomical Journal AN = Astronomische Nachrichten APJ = Astrophysical Journal APJS = Astrophysical Journal Supplement Series CAPE = Annals of Cape Observatory DAO = Publications of the Dominion Astrophysical Observatory DDO = Publications of the David Dunlap Observatory GOTT = Astronomische Mitteilungen Koenigliche Sternwarte Goettingen LOB = Lick Observatory Bulletin MEM = Memoirs of the Royal Astronomical Society MEMRA= Memoirs of the Royal Astronomical Society MN = Monthly Notices of the Royal Astronomical Society MNRAS= Monthly Notices of the Royal Astronomical Society PAO = Publications of the Allegheny Observatory PASP = Publications of the Astronomical Society of Pacific PDAO = Publications of the Dominion Astrophysical Observatory PDO = Publication of the Dominion Observatory PLO = Publications of the Lick Observatory POCP = Publications Observatoire Central Pulkovo Serie II POHP = Publications de l'Observatoire de Haute-Provence PULK = Mitteilungen Nikolai-Hauptsternwarte Pulkowo PUM = Publications of the Observatory of the University of Michigan PYO = Publications of the Yale Observatory RASC = Journal of the Royal Astronomical Society of Canada ROB = Royal Observatory Bulletin --- Francois Ochsenbein CDS 1995 Jan 19 III_55.xml A Catalogue and Bibliography of Mn-Hg Stars 3059 III/59 Catalogue and Bibliography of Mn-Hg Stars A Catalogue and Bibliography of Mn-Hg Stars H Schneider CDS Bull. No. 20, p. 113 ??? ??? 1981 1981BICDS..20..113S Bibliography Stars, Ap Stars, peculiar In the present catalogue all Ap stars of the type Mn-Hg, Mn or Hg are summarized. Also, the stars which are suspected to be of this type are included. If in the literature two or more classifications of a star indicate the same type (or one with high dispersion) it is listed as of known type. If only doubtful or different classifications exist for a star, it is indicated as suspected.
Data file (Table 1) HD HD (Cat. <III/135>) number --- HR Bright Star (HR, Cat. <V/50>)) number --- Name Common name --- mv Visual magnitude from SAO catalog mag Sp Spectral type from SAO catalog --- dupl Duplicity code D = Double SB = Spectroscopic binary SB1 + 1-line system SB2 = 2-line system V = Visual binary. The following number indicates the number of components, the following letter, the component which is the Ap star (E.g. V3B) --- RAh Right ascension (1950) - hour The positions are taken from the SAO Catalog. h RAm Right ascension (1950) - minutes min RAs Right ascension (1950) - seconds s DE- Declination sign --- DEd Declination degrees (1950) deg DEm Decliantion minutes (1950) arcmin DEs Decliantion seconds (1950) arcsec n_Sp Suspected Mn-Hg star or misc. cl. --- group indicates member of group/cluster or misc. remark (see remarks.dat) --- ref References - see refs.dat --- Remarks for data in table 1 HD HD designation, as in data.dat --- Text Text of remark --- *Bibliography (Table 4) ID Reference number ID is repeated when the reference requires more than one line. --- Text Reference Books are indicated by ' ' in this file, remarks.txt, and abrev.txt. See file "abrev.txt" for abbreviations of magazines. --- abrev.txt Abbreviations used in refs.dat N. G. Roman and Julie Anne Watko SSDOO/ADC 1997 Nov 07 III_59.xml Revised Catalogue of Stellar Rotational Velocities 3063B III/63B Revised Catalogue of Rotational Velocities Revised Catalogue of Stellar Rotational Velocities A Uesugi I Fukuda Department of Astronomy, Kyito Univ., Japan ??? ??? 1982 1982csrv.book.....U Rotational velocities The machine-readable "Revised Catalogue of Stellar Rotational Velocities" provides mean v.sin(i) data on the old Slettebak system (Slettebak 1949, 1954, 1955, 1956; Slettebak and Howard 1955) for 6472 stars. The catalog results from the review, analysis and transformation of 11460 data from 102 sources. Included in the computerized version are star identification (major catalog number, name if the star has one, or cluster identification, etc.), a mean projected rotational velocity, and a list of source references. This version of the machine-readable catalog is comprehensive and supersedes the earlier compilation of Uesugi and Fukuda (1970).
The Catalogue of Rotational Velocities HD Henry Draper Catalog (HD) number --- m_HD HD component letters or additional numbers --- Name Common name of the object number=1 Name of star, e.g. Flamsteed and/ or Bayer designation and constellation abbreviation, variable-star name, cluster identification and number, Durchmusterung number for non-HD stars. Parenthesized letters denote lower case. --- l_RotVel Indicates RotVel is upper/lower limit --- RotVel Projected rotational velocity, v.sin(i) km/s u_RotVel ':' if RotVel uncertain, '::' if very uncertain --- NumObs Number of observations, continued with A=10; B=11; C=12, etc. --- Ref1 Reference code (see refs) --- Ref2 Reference code (see refs) --- Ref3 Reference code (see refs) --- Ref4 Reference code (see refs) --- Ref5 Reference code (see refs) --- Ref6 Reference code (see refs) --- Ref7 Reference code (see refs) --- Ref8 Reference code (see refs) --- Ref9 Reference code (see refs) --- Ref10 Reference code (see refs) --- Ref11 Reference code (see refs) --- Ref12 Reference code (see refs) --- The References RefCode Reference code from table RotVel_Data (blank for continuation lines) --- Text Reference --- Francois Ochsenbein CDS 1995 Sep 08 Appreciation is expressed to K. Sadakane of Osaka University for personally transmitting our request for a copy of the tape to the Astronomical Data Center, Japan, and to Y. Terashita and A. Hayashi for preparing and supplying the magnetic tape. UNKNOWN UNKNOWN * October 1982, ADC/NSSDC (Wayne H. Warren Jr.) A magnetic tape containing the "Revised Catalogue of Stellar Rotational Velocities" was received from the Astronomical Data Center, Japan, on 4 March 1983. Minor modifications, as described below, were made to the data file in order to effect a more homogeneous format consistent with other computerized catalogs. 1. The HD field contained a zero for every non-HD star; these were converted to blanks. 2. The abbreviations "BD", "CD", and "CP" were added to Durchmusterung (DM) numbers where they were absent. The abbreviation CP already occurred for CPD stars in the zones -22 degrees to -52 degrees where CD numbers are ordinarily used (following the HD convention). An unknown character (not in the published version) occurred in the Name field after all zone numbers for DM identifications. All occurrences of this character were changed to blanks. * October 1991: catalogue prepared (Lee E. Brotzmann) for the "Selected Astronomical Catalogs" Vol. 1 CD-ROM, directory: /spectro/rotvel * September 1995: catalogue documentation standardized at CDS III_63B.xml Calalog of Be Stars 3067A III/67A Catalogue of Be stars Calalog of Be Stars M Jaschek D Egret IAU Symp. 98 261 1982 1982IAUS...98..261J Stars, Be The catalog is a compilation of about 1100 Be stars. The definition of a Be star in the catalog is that of a non-supergiant B star that has shown emission in one Balmer line at least once. For this reason, with one exception, all stars for which no MK classification exists have been excluded, as have planetary nebulae and spectroscopic binaries. It is important to note that MK types are established in a wavelength region in which H-alpha is not included. Therefore, many stars having H-alpha in emission are classified as normal stars, being called, for instance, B3 V, not B3 Ve. The catalog includes DM and HD identifications, numbers in the main lists of emission- line stars, coordinates, V magnitudes and UBV photometry (when available from Nicolet's (1978) compilation), adopted MK classifications, radial velocities, rotational velocities, and bibliographical references in a separate file.
The catalogue with additional data Number DM or CSI number --- BeStar Be star number from MWC, AS, or Henize --- HD Henry Draper Catalog (HD) number --- RAh Hours RA, equinox B1950 h RAm Minutes RA, equinox B1950 min RAs Seconds RA, equinox B1950 s u_RAs Uncertainty flag (:) to indicate uncertainty in the coordinates --- DE- Sign Dec, equinox B1950 --- DEd Degrees Dec, equinox B1950 deg DEm Minutes Dec, equinox B1950 arcmin DEs Seconds Dec, equinox B1950 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Vmag V magnitude in the UBV system mag u_Vmag Uncertainty flag (:) on Vmag; also set when Vmag not in standard UBV system --- n_Vmag 'V' for variable, 'D' for integrated magnitude of binary --- r_Vmag '*' if V from CSI; else V from Nicolet (1978) --- q_Vmag V quality number=1 photometric quality from 1 (poor) to 4 (very good); record number 82 (MWC 445) has the undefined character 'E' in the field record number 827 (CD-4410889) has the undefined character ':' --- B-V B-V color in the UBV system mag q_B-V B-V quality number=1 photometric quality from 1 (poor) to 4 (very good); record number 82 (MWC 445) has the undefined character 'E' in the field record number 827 (CD-4410889) has the undefined character ':' --- U-B U-B color in the UBV system mag q_U-B U-B quality number=1 photometric quality from 1 (poor) to 4 (very good); record number 82 (MWC 445) has the undefined character 'E' in the field record number 827 (CD-4410889) has the undefined character ':' --- RadVel Radial velocity km/s q_RadVel Radial velocity quality, from 'A' (very good) to 'E' or 'F' (very poor) --- Disp Dispersive system used to determine SpType (see doc.) --- SpType Spectral type --- RotVel Projected rotational velocity, v sin i km/s e_RotVel Probable error in RotVel km/s BinFlag '*' if object is visual binary from ADS or IDS --- SBFlag '*' if object is spectroscopic binary with known orbit --- uvbyFlag '*' if there is uvby data available --- 10ColFlag '*' if there is UBVRIJKLMN data available --- UVFlag '*' if object in Celescope Catalogue --- Name Bayer-Flamsteed designation --- VarName Variable star identification --- adc.doc ADC Document from CD-ROM by Anne C. Raugh adc.tex ADC Document from CD-ROM (LaTeX) Francois Ochsenbein CDS 1996 Sep 26 UNKNOWN UNKNOWN * Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory: /spectro/bestars * 13-Jan-1995: modifications at CDS - the two data files have been merged into a single one. - RA has been rewritten in a standard form (some values had format F4.1 in "RAm" column) III_67A.xml A List of Early-Type Chemically Peculiar Stars 3068 III/68 List of Early-Type Chemically Peculiar Stars A List of Early-Type Chemically Peculiar Stars D Egret M Jaschek Comptes Rendus Symp. Liege No. 23, p. 495 ??? ??? 1981 1981cpsu.conf..495E Stars, early-type Abundances, peculiar Stars, peculiar This catalogue is a subset of the "CATALOGUE OF STELLAR GROUPS" (CSG, Jaschek M. and Egret D., 1981). It provides a list of identifications, positions, UBV photometry, subgroup and references for chemically peculiar stars corresponding to the following groups: TABLE 1: Helium abnormal stars TABLE 2: Ap stars TABLE 3: Am stars A bibliography file is also included.
Group 1: Helium abnormal stars Group 2: Ap stars Group 3: Am stars ID Star identification (HD or DM) --- RAh Right Ascension (1950) hours h RAm Right Ascension (1950) minutes min RAs Right Ascension (1950) seconds s n_RAs Note on RAs * = RA was originally given to 0.1 minute. To homogenize the data format, RA values were converted to seconds at ADC. RA values in these records are only accurate to 6 seconds; therefore, the decimal place is omitted. blank = RA was originally given to 0.1 second or is omitted. --- DE- Declination (1950) sign --- DEd Declination (1950) degrees deg DEm Declination (1950) arcminutes arcmin DEs Declination (1950) arcseconds arcsec Glon Galactic Longitude deg Glat Galactic Latitude deg V V magnitude mag q_V Quality index on V A = best D = worst : = uncertain --- paren1 Parentheses --- B-V B-V color index mag paren2 Parentheses --- q_B-V Quality index on B-V A = best D = worst : = uncertain --- U-B U-B color index mag q_U-B Quality index on U-B A = best D = worst : = uncertain --- Sub Indication of subgroup The "helium abnormal stars" are B-type stars having either strong He lines (subgroup a) or weak He lines (subgroup c). Not included in this list are He-strong stars of Pop. II (extreme helium stars of Hunger), subdwarfs and objects like Ups Sgr. Stars being known as spectroscopic or photometric (or both) variables are flagged with a "v". The "Ap stars" are B or A type stars with abnormally intensified lines of different elements. Because of the sometimes conflicting subgroup assign- ments, only four subgroups have been retained. 1 = Si and Si L4200 stars 2 = Hg, Mn and Hg-Mn stars 3 = Si combined with Cr, Eu, Sr, etc. (i.e. SiCr, SiEu, SiSr or SiCrEu) 4 = Cr, Eu, Sr and combinations (i.e. CrEu, Cr, CrEuSr, etc.) The "Am stars" are A or early F type stars, in which the Balmer lines, the CaII lines and the metallic lines do not correspond to a unique spectral type. No spectral classification of these stars is provided here. The reader is referred to Curchod and Hauck (1979) for detailed classifi- cations, when available. --- uvby Indicates existence of Stroemgren photometry --- CSI CSI Identification: I3, I5, I2 --- ref Reference for assignment of peculiarity group --- References ref Reference number If ref is blank, then text is continued from previous record. --- text Text of reference --- Julie Anne Watko SSDOO/ADC 1996 Aug 21 III_68.xml A Catalog of 0.2-A Resolution Far-Ultraviolet Stellar Spectra Measured with Copernicus 3077 III/77 Copernicus 0.2-A Resolution Far-UV Stellar Spectra A Catalog of 0.2-A Resolution Far-Ultraviolet Stellar Spectra Measured with Copernicus T P Snow Jr. E B Jenkins Astrophys. J. Suppl. 33 269 1977 1977ApJS...33..269S http://iuewww.gsfc.nasa.gov/copernicus/oao3.html : data in FITSBohlin, R.C. 1975, ApJ, 200, 402. (1975ApJ...200..402B) Spectrophotometry Spectra, ultraviolet The catalog is a subset comprising data for 60 O- and B-type stars observed by the Copernicus satellite. For each star a FITS file was created of the observed spectrum. Each spectrum has 2250 photometric data points. The wavelength range is from 1000 to 1450 Angstroems in 0.2-Angstrom steps. The data were acquired with photomultiplier U2, which had a nominal bandpass of 0.2 Angstrom (A) and scanned the spectrum with a 0.2 A step length, integrating for 13.6 sec at each wavelength position.
Copernicus
Basic data of observed stars FileName Name of file (in this directory) with spectrum --- HR Harvard Revised (Bright Star) number number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> --- Name Current designation of the star number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> --- HD Henry Draper (cat. <III/135>) designation number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> --- RAh Right Ascension J2000 (hours) number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> h RAm Right Ascension J2000 (minutes) number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> min RAs Right Ascension J2000 (seconds) number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> s DE- Declination J2000 (sign) number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> --- DEd Declination J2000 (degrees) number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> deg DEm Declination J2000 (minutes) number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> arcmin DEs Declination J2000 (seconds) number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> arcsec Vmag Visual magnitude number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> mag B-V Colour index number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> mag SpType Spectral type number=1 These values were extracted from the Bright Star Catalog, 5th Revised Edition by D. Hoffleit and W. Warren H. Jr, 1991, catalog <V/50> --- Spectrum of Zeta Pup Spectrum of 9 Sgr Spectrum of 29 CMa Spectrum of Xi Per Spectrum of HD 199579 Spectrum of 15 Mon Spectrum of Theta 1 Ori C Spectrum of Lambda Ori A Spectrum of Tau CMa Spectrum of Iota Ori Spectrum of 10 Lac Spectrum of Alpha Cam Spectrum of Delta Ori A Spectrum of Zeta Oph Spectrum of Mu Col Spectrum of Mu Nor Spectrum of Zeta Ori A Spectrum of Epsilon Ori Spectrum of Tau Sco Spectrum of Kappa Ori Spectrum of Epsilon Per Spectrum of Delta Sco Spectrum of Theta Car Spectrum of Rho Leo Spectrum of Gamma Ara Spectrum of Zeta Per Spectrum of 139 Tau Spectrum of Beta CMa Spectrum of Beta Cen A Spectrum of Sigma Sco Spectrum of Omicron Per Spectrum of 40 Per Spectrum of Alpha Vir Spectrum of 42 Ori Spectrum of Pi Sco Spectrum of Lambda Sco Spectrum of Epsilon CMa Spectrum of Gamma Peg Spectrum of Upsilon Sco Spectrum of Zeta Cen Spectrum of Sigma Sgr Spectrum of Alpha Pav Spectrum of Omicron2 CMa Spectrum of Iota Her Spectrum of Eta UMa Spectrum of HD 21278 Spectrum of Eta CMa Spectrum of 67 Oph Spectrum of Delta Per Spectrum of Zeta Dra Spectrum of Alpha Col Spectrum of Eta Tau Spectrum of Phi Eri Spectrum of Alpha Gru Spectrum of Alpha Leo Spectrum of Beta Ori A Spectrum of 20 Tau Spectrum of Beta Lib Spectrum of Alpha Lyr Spectrum of Alpha CMa A wave Wavelength in nm number= From these two numbers we can estimate the noise in the spectrum, i.e., (COUNTS/N_S)**(1/2), where COUNTS ~= 1.5*S + 40 (Bohlin 1975), is the total observed (namely, uncorrected) count rate. This was done for the good data points. nm S average corrected signal counts per 14 seconds number= From these two numbers we can estimate the noise in the spectrum, i.e., (COUNTS/N_S)**(1/2), where COUNTS ~= 1.5*S + 40 (Bohlin 1975), is the total observed (namely, uncorrected) count rate. This was done for the good data points. 0.0714/s o_S number of observations per wavelength point number= From these two numbers we can estimate the noise in the spectrum, i.e., (COUNTS/N_S)**(1/2), where COUNTS ~= 1.5*S + 40 (Bohlin 1975), is the total observed (namely, uncorrected) count rate. This was done for the good data points. --- ERR Error Flag: 1 = good; 0 = blank data; -1 = S negative; -2 = OBS = zero; -3 = OBS overflow OBS > 9, data lost number= From these two numbers we can estimate the noise in the spectrum, i.e., (COUNTS/N_S)**(1/2), where COUNTS ~= 1.5*S + 40 (Bohlin 1975), is the total observed (namely, uncorrected) count rate. This was done for the good data points. --- COUNTS =-9.990E+01 uncorrected count rate From these two numbers we can estimate the noise in the spectrum, i.e., (COUNTS/N_S)**(1/2), where COUNTS ~= 1.5*S + 40 (Bohlin 1975), is the total observed (namely, uncorrected) count rate. This was done for the good data points. number= From these two numbers we can estimate the noise in the spectrum, i.e., (COUNTS/N_S)**(1/2), where COUNTS ~= 1.5*S + 40 (Bohlin 1975), is the total observed (namely, uncorrected) count rate. This was done for the good data points. --- e_COUNTS =-9.990E+01 noise in observed counts number= From these two numbers we can estimate the noise in the spectrum, i.e., (COUNTS/N_S)**(1/2), where COUNTS ~= 1.5*S + 40 (Bohlin 1975), is the total observed (namely, uncorrected) count rate. This was done for the good data points. --- Paul Kuin Hughes STX/NASA 1997 Aug 07 The original ADC documentation by William T. Sheridan and Wayne H. Warren Jr. (1981) and the ApJS publication (Snow and Jenkins, 1977) were used to generate this ReadMe file. UNKNOWN UNKNOWN * A magnetic tape containing the far-ultraviolet spectral data was received from Dr. Edward B. Jenkins in June 1979. This tape was formatted as a print tape having the record structure and spacing of the printed pages in the Snow and Jenkins (1977) paper. Due to programming complications arising from the original format, which contains blank lines and data fields for many stars within each logical record, it was decided to rewrite the tape to a more suitable format for data analysis and plotting purposes. Thus, the tape was converted at the Astronomical Data Center to the format contained in the previous catalog data, catalog.ori, where the data fields and slash characters remain identical to those used in the published tables. One more reformatting round was done to bring the data format in line with other standardized catalogs. This work was started by J. Lyu and completed by P. Kuin. An error in the number of observations field, that was allowed only one character during the previous reformatting, was found. There appears to have been a number of data points with more than 9 observations. These numbers were lost. For the reformatted files the number has been set to 10 and an error flag has been added to identify the record. The data were converted by P. Kuin into separate files that can be easily converted to the FITS format using the tofits program. * 20-May-1998: the file "stars.dat" containing basic data of the observed stars was added at CDS (F. Ochsenbein) UNKNOWN UNKNOWN Brief description of catalog.ori: If space is at a premium, the original data file prepared by the ADC is still available. All the spectra, including the number of observations, are in this file. The format of the file is a block of 151 records for each object: Record 1 contains the object identification in the first 16 bytes. Records 2-151 contain the spectral data, 15 data points per record. Each data point consists of two numbers and is of the form: S/Obs == Average Corrected Signal/Number of Observations, in format (I6,1H/,I1) or blank. Note that S is the corrected signal in counts per 14s and that Obs is the number of observations that were averaged together to determine S. From these two numbers we can estimate the noise in the spectrum, i.e., (S'/Obs)**(1/2), where S' ~= 1.5*S + 40 (Bohlin 1975), is the total observed (namely, uncorrected) count rate. If a data point is blank, it was deleted from the originally published results because of an obvious flaw attributable to guidance errors or to overcorrection or undercorrection for particle background. Since data fields can contain blanks and zeroes (see the data tables and associated graphical spectra in Snow and Jenkins 1977) which indicate that they should not be used, the 'number of observations' field must be checked for zero before using a data point. III_77.xml MK Classification Catalogue Extension 3078 III/78 MK Classification Extension MK Classification Catalogue Extension P M Kennedy Mt Stromlo & Siding Spring Observatories, Australia ??? ??? 1983 1983 III/18 : Stellar Spectra classified in the MK system (Jaschek+, 1963) III/42 : Selected MK Spectral Types (Jaschek, 1978) III/189 : General Catalogue of MK types (Buscombe, 1995) Jaschek, C., Conde, H. and de Sierra, A.C. 1964, "Catalogue of Stellar Spectra Classified in the Morgan-Keenan System", Publ. La Plata Obs., Ser Astron. 28, No. 2. (CDS Cat. <III/18>) Morgan, W.W. and Keenan, P.C. 1973, Annual Rev. Astron. Astrophys. 11, 29. MK spectral classification The catalog provides classifications on the Morgan-Keenan (MK) system published in the literature since the appearance of the La Plata catalog (Jaschek et al., 1964). In addition to the MK types, the catalog contains, for REFERENCE PURPOSES ONLY, UBV photometry, some component identifications for multiple systems, and miscellaneous remarks, e.g., cluster membership, although this information is not professed to be complete. A second file of the machine version contains the bibliographical references cited in the data file and indicates classifications done by objective-prism techniques (OP) or from photometric studies (PHOT). Note that extragalactic stars (e.g. in LMC, SMC) are not included.
The Catalogue Name Object identification number=1 Entries are ordered in the catalog with the following priority: HD numbers in ascending numerical order; HDE numbers in ascending numerical order; DM numbers in descending zone and increasing numerical order; Other designations use the following acronyms: BB see Bok & Basinski, Mem. Mt. Stromlo Obs No 16, 1964 BS see Stenholm (1975A&A....39..307S) LF5 see McCuskey and Houk, (1964AJ.....69..412M) LFS see Smith, (1968MNRAS.138..109S) LS I Luminous Stars in the Northern Milky Way I , cat. <III/76> LYNGA see Ark.f.Astr., 3, No.8 MCP McCormick Proper Motion Areas - McCormick Publs 7 and 10 MS see MacConnell & Sanduleak (1970PASP...82...80M) RWT see reference#361 (1979AJ.....84..534C), 1971AJ.....76.1099R and 1974AJ.....79.1406R SW see reference#330 (1977A&AS...27..403S) W see reference#301 (1976A&AS...26...31W) WRA see reference#301 (1976A&AS...26...31W) --- RAh Right Ascension 2000 (hours) number=2 the position may be very rough, or even inexistant. h RAm Right Ascension 2000 (minutes) number=2 the position may be very rough, or even inexistant. min DE- Declination 2000 (sign) number=2 the position may be very rough, or even inexistant. --- DEd Declination 2000 (degrees) number=2 the position may be very rough, or even inexistant. deg DEm Declination 2000 (minutes) number=2 the position may be very rough, or even inexistant. arcmin SpType MK spectral type number=3 The W in Wolf-Rayet types will be found in byte 31, as will a left parenthesis for uncertain types. The temperature class is in byte 32, but other characters are also there, e.g. P (peculiar), the D in Delta DEL types, etc.; the temperature subclass is in bytes 34-36, but other characters can be there too. Bytes 37-43 contain luminosities, peculiarities, etc. --- r_SpType Reference number for the MK type number=4 Three stars have no reference for the spectral type: HD 62318 (record#8104), HD 175253 (record#19457) and HD 222872B (record#23441) --- Vmag V magnitude as taken from the literature. mag n_Vmag V if V variable, : for uncertain --- B-V B-V color. Plus signs are omitted. mag U-B U-B color. Plus signs are omitted. mag r_Vmag Reference number for photometry. --- Rem Remarks. number=5 Remarks can be component identification, variable-star names, cluster membership, HDE numbers (6 digits), miscellaneous identifications. Byte 80 contains an asterisk for stars classified by Morgan and Keenan (1973) for the revised MK system. --- The References Ref Reference number, as written in columns r_SpType and r_Vmag of the catalog --- BibRef Bibliographic Reference --- Auth Authors --- Note List, or type of classification like OP for objective-prism classification, PHOT for photometric classification --- Francois Ochsenbein CDS 1996 Dec 23 UNKNOWN UNKNOWN The machine-readable MK Classification Extension Catalogue, version 1983 was received at CDS in 1983; a first documentation was prepared at NASA/ADC by Wayne H. Warren. The catalogue was checked against catalogue standards at CDS in December 1996: several misalignments, missing decimal points, etc were corrected. III_78.xml A Photometric Atlas of the Spectrum of Gamma Tauri 5186-8700 A 3079A III/79A Atlas of the Spectrum of Gamma Tauri, 5186-8700 A A Photometric Atlas of the Spectrum of Gamma Tauri 5186-8700 A L Appelquist J Andersen W A Fisher J M Fletcher P Kjaergaard A&AS 52 237 1983 1983A&AS...52..237A Spectrophotometry Stars, K-type Stars, giant The Photometric Atlas of the Spectrum of gamma Tauri 5186-8700 angstroms (gamma TAU; Appelquist et al. 1983) lists normalized intensity and wavelength at 22,725 points along the spectrum of the K giant gamma Tauri. This atlas supplements the atlas already completed for the blue-green region by Gratton et al. ( 1975). The atlas is "based on spectrograms of dispersion 4.9 angstroms/mm obtained with the 1.2m telescope and coude spectrograph of the Dominion Astrophysical Observatory" (Appelquist et al. 1983) and is the first of a set of four (including alpha Boo, rho Boo, and delta Boo A) intended to illustrate the effects of temperature and metal abundance variations on the spectrum. The catalog is in five files: the first four files cover the ranges 5186-6004, 6000-7004, 7000-8004, and 8000-8700 angstroms, respectively, and the fifth file lists the entire range without gaps or overlap.
5185-6005 A 6000-7004 A 6999-8004 A 7999-8700 A 5185-8700 A Wavelen1 Wavelength in angstroms 0.1nm Inten1 Intensity mag Wavelen2 Wavelength in angstroms 0.1nm Inten2 Intensity mag Wavelen3 Wavelength in angstroms 0.1nm Inten3 Intensity mag Wavelen4 Wavelength in angstroms 0.1nm Inten4 Intensity mag C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 22 UNKNOWN UNKNOWN The Photometric Atlas of the Spectrum of gamma Tauri 5186-8700 A (gamma TAU) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques de Strasbourg (CDS), in September 1983. The catalog was in five text files, formatted as described above. Eight bytes on the beginning of each record containing the file identification were removed, and trailing blanks were trimmed by means of an editor to reduce the record size from 76 to 68 bytes. A FORTRAN program was run to check the validity of each field according to its data type and value. The original documentation was scanned and incorporated into this ReadMe file. No attempt has been made to reorganize the data. Currently four data points are on each record. III_79A.xml Catalogue of two-dimensional spectral types for the HD stars. Vol.3 3080 III/80 Michigan Catalogue of HD stars, Vol.3 Catalogue of two-dimensional spectral types for the HD stars. Vol.3 N Houk Ann Arbor, Dept. of Astronomy, Univ. of Michigan ??? ??? 1982 1982MSS...C03....0H III/31B : Volume 1 of this catalog (additional declination zones) III/51B : Volume 2 of this catalog (additional declination zones) III/133 : Volume 4 of this catalog (additional declination zones) MK spectral classification Plate data Spectral types The catalog contains spectral types for the HD stars from declinations -40 to -26 deg. The stars were classified visually by N. Houk on objective-prism plates taken at a dispersion of 108 A/mm with a resolution of about 2 A/mm. The only difference in form between this volume and Volume 2 is that Smithsonian Astrophysical Observatory Star Catalog (SAO) numbers are given instead of Cape Photographic Durchmusterung (CPD) numbers. The catalog also includes photographic magnitudes, right ascension and declination (B1900.0), precession, galactic coordinates, and cross identifications to the numbering systems of the Cordoba Durchmusterung and SAO.
The Catalogue (vol.3) HD Henry Draper Catalog (HD) number --- Case * = sp. type lower case in printed ver. --- n_SpType + if spectral type is from HD Catalog --- SpType Spectral type --- Ave_Flag A = classification used is an average. --- q_SpType Quality of the classification, see adc.doc --- Remark Remark (see adc.doc Table 5 for description) --- Ptg Photographic magnitude from HD catalog mag Var_Flag 'V' if star is known or suspected variable --- RAh Hours RA, epoch 1900.0 h RAm Minutes RA, epoch 1900.0 min RAs Seconds RA, epoch 1900.0 s FlagPos the '*' indicates a position known to an arc-minute --- DE- Sign Dec, epoch 1900.0 --- DEd Degrees Dec, epoch 1900.0 deg DEm Minutes Dec, epoch 1900.0 arcmin DEs Seconds Dec, epoch 1900.0 (blank if FlagPos is flagged with '*') arcsec precRAm Centennial precession in RA, minutes 0.01min/yr precRAs Centennial precession in RA, seconds 0.01s/yr FlagPrec * if precession in RA is given to 0.1 minutes/century in the published catalog. --- precDE- Centennial precession in Dec, sign 0.01arcmin/yr precDEm Centennial precession in Dec, minutes 0.01arcmin/yr precDEs Centennial precession in Dec, seconds 0.01arcsec/yr GLON Galactic longitude deg GLAT Galactic latitude deg CD Cordoba Durchmusterung identification (CD-ZZNNNNN) --- SAO SAO Catalog number --- Plate1 Plate code #1 (see file plates.dat) --- Plate2 Plate code #2 (see file plates.dat) --- Plate3 Plate code #3 (see file plates.dat) --- Plate4 Plate code #4 (see file plates.dat) --- Remarks to Vol.3 HD Henry Draper Catalog (HD) number --- Remark Remarks in free form text --- List of plates Code Plate code --- Number Plate Number --- Date Exposure date --- adc.doc Documentation by Robert S. Hill Francois Ochsenbein CDS 1994 Dec 08 UNKNOWN UNKNOWN * 09-Nov-1993: list of plates added at CDS * 08-Dec-1994: list of plates corrected by Shiro Nishimura [ADAC/NAOJ] III_80.xml IUE Low-Dispersion Spectra Reference Atlas. I. Normal Stars 3083 III/83 IUE Low-Dispersion Reference Atlas I, Normal Stars IUE Low-Dispersion Spectra Reference Atlas. I. Normal Stars A Heck D Egret M Jaschek C Jaschek Astron. Astrophys. Suppl. Ser. 57 213 1984 1984A&AS...57..213H Spectrophotometry Spectra, ultraviolet The atlas contains the fluxes (2 angstroms/step) of 229 low-dispersion stellar spectra collected by the International Ultraviolet Explorer (IUE) satellite, compiled for the purpose of establishing reference spectral sequences in the ultraviolet range. The sequences have been constructed and the standard stars selected directly from the ultraviolet material, staying as far as possible within the general MK frame. The catalog is essentially composed of stars exhibiting normal behaviour in the ultraviolet. A few peculiar objects have, however, been included as an illustration of typical abnormalities. This work clearly pointed out the dangers of extrapolating a spectral classification based on a given wavelength range to another one, and, in particular, of using the MK spectral type alone outside its definition range.
IUE
Calibrated fluxes for each source ID Identification of the star (preferably HD) Each star occupies 205 records of the catalog. ID is repeated. For a list of the sources in order of appearance in this file, please see sources.dat. --- Fmax Maximum flux on plot Value used as maximum on the y-axis when plotting the spectrum for the atlas. Repeated on each line for same star. (unit : 10-14 erg cm-2 A-1 s-1) 10-17W/m2/A Num Record number for the star --- Lambda Wavelength for first flux value in record 0.1nm Flux1 Calibrated absolute fluxes (erg s-1 cm-2 A-1) Each star has fluxes given for wavelengths 1153A to 3201A stepped by 2A. Five fluxes are given per record. The 205 records for each star are labeled in the Num field. mW/m2/A Flux2 Flux for ({Lambda} + 2A) mW/m2/A Flux3 Flux for ({Lambda} + 4A) mW/m2/A Flux4 Flux for ({Lambda} + 6A) mW/m2/A Flux5 Flux for ({Lambda} + 8A) mW/m2/A List of sources RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec ID Identification of the star (preferably HD) --- Fmax Maximum flux on atlas plot of spectrum 10-17W/m2/Angstroem Julie Anne Watko SSDOO/ADC 1997 Jan 02 UNKNOWN UNKNOWN Francois Ochsenbein [CDS] 03-Dec-1993 The original file has been transformed to allow easier computer reading: the redundant 1025 wavelength values (1153 to 3201 stepped by 2) were removed, floating-point numbers were normalized with the addition of the "E" between the mantissa and the exponent. Julie Anne Watko [ADC] 02-JAN-1997 The data file had been formatted with one line per star. The old 10270 byte records were difficult to read on some computers. Fluxes were reformatted to accommodate an 80 byte logical record length. Running numbers and wavelengths were added. sources.dat was created, and the Intro document from CDS was updated. The 2000-position of stars was added at CDS (F.O., 08-Oct-1997) III_83.xml Catalogue of Galactic O Stars 3084B III/84B Galactic O Stars Catalogue of Galactic O Stars C Cruz-Gonzalez E Recillas-Cruz R Costero M Peimbert S Torres-Peimbert Rev. Mex. Astron. Astrof. 1 211 1974 1974RMxAA...1..211C Stars, O The catalog is a compilation of published data for 644 galactic O stars of luminosity V. The catalog is intended to be useful to O-type star observers by providing a reference list for general studies on O-type stars. The catalog includes cross identifications, equatorial and galactic coordinates, visual or photographic magnitudes, B-V, spectral types, distances to the stars, radial velocities, H II region identifications, remarks, and notes.
Catalog Data CGO CGO number Sequential number of the object in this catalog --- Ident Alternate ident --- RAh Right Ascension 1975.0 (hours) Equatorial coordinate for Equinox 1975.0 h RAm RA in minutes min DE- Sign of Declination 1975.0 --- DEd DEC degrees deg DEm DEC arcminutes arcmin GLONd Galactic longitude degrees Galactic coordinate (l II and b II) deg GLONm Galactic longitude arcminutes arcmin GLATsign Galactic latitude sign --- GLATd Galactic latitude degrees deg GLATm Galactic latitude arcminutes arcmin Mag magnitudes V in the UBV system where available, otherwise the photographic magnitude (see mag. quality index) mag q_Mag Mag. quality index Single-character code indicating the quality of the magnitude. The following codes are used: P The magnitude is photographic rather than visual. These stars will not have B-V listed. V The star is an intrinsic variable. M The star is one component of a close multiple system. The magnitude listed may be contaminated because of "the brightness of the companion (delta_m < 2) and its proximity (d < 10")." C A correction has been applied to allow for a companion. In these cases delta_m is given in the remarks following "SB" or "VB": The value given for delta_m is the magnitude difference between the O star and its companion, as given in the literature. The magnitude listed in the CGO corresponds to the observed visual intensity from which the intensity of the companion has been subtracted. ? The magnitude is not known. The magnitude field will be blank. --- B-V B-V magnitudes mag Sp Spectral type --- q_Sp Spec. type qual. ind. Spectral type quality index -- Single-character code indicating the quality of the spectral index. Cruz-Gonzlez et al. (1974) define the following codes for this field: H High quality. This is assigned only to spectral types from the following sources: Conti, P. S. 1973a, Astrophys. J., 179, 161. Conti, P. S. 1973b, Astrophys. J., 179, 181. Conti, P. S. 1974, Astrophys. J., 187, 539. Conti, P. S. and Alschuler, W. R. 1971, Astrophys. J., 170, 325. Humphreys, R. M. 1970, Astron. J., 75, 602. Humphreys, R. M. 1973, Astron. Astrophys. Suppl. Ser., 9, 85. Walborn, N. R. 1971, Astrophys. J. Suppl. Ser., 23, 257. Walborn, N. R. 1972, Astron. J., 77, 312. Walborn, N. R. 1973a, Astron. J., 78, 1067. Walborn, N. R. 1973b, Astrophys. J., 179, 517. M Medium quality. This index is assigned to spectral types determined by authors other than those listed above with at least two coincident spectra. L Low quality. This index is assigned to spectral types for which there is either only one determination, disagreement in the literature, or acknowledged doubts. N This index is assigned to spectral types for which there is either no luminosity class or widely different luminosity classes. --- D-star Distance to star Distance to the star in kiloparsecs. For stars in clusters this is just the distance to the cluster. For stars not in a cluster a distance was calculated using the photometric data and luminosity class where available, or the photographic magnitude and an assumed reddening of 1 mag/kpc. kpc q_D-star Distance qual. index Single-character code indicating the quality of the distance in bytes 75-80. This quality depends on the spectral type quality index, the magnitude quality index, and the method of distance determination (see Table below). Table. Magnitude Quality Index Definition Quality Spectral Magnitude Distances Index Index Index Determination A from cluster B H blank or C photometric C H V or M photometric D M blank or C photometric E M V or M photometric F L blank or C photometric G L V or M photometric H H P (Av = l mag/kpc) I L P (Av = 1 mag/kpc) J M P (Av = l mag/kpc) K N blank or C (lum. class V) L N V or M (lum. class V) Av = assumed normal reddening law, Av = 3E(B - V) Luminosity class V assumed for those stars with no published luminosity class --- D-Gal-P Distance to galactic plane Perpendicular distance from the star to the galactic plane in parsecs pc Vsun Hel. radial velocity Heliocentric radial velocity of the star in km/sec. See Cruz-Gonzalez et al. (1974) for a discussion of how this value was determined and the assignment of the corresponding quality index. km/s q_Vsun Hel. RV quality index Single-character code indicating the quality of the heliocentric radial velocity. The following codes are used: A Emax = 4 km/s B Emax = 6 km/s C Emax = 9 km/s D Emax = 20 km/s For spectroscopic binaries with known orbital elements, the quality index assigned is the same as that of Batten (1967). "In the very few cases where the quality according to Batten (1967) was 'E', which was changed to 'D' unless the orbit was a provisional one." --- VLSR Rad. vel. (LSR) Radial velocity of the star with respect to the local standard of rest (LSR), in km/sec. The heliocentric radial velocities ... of the start were reduced to the LSR assuming the solar motion obtained by Woolley, Epps, Penston, and Pocock (1970) for the local stars; namely, u = 10 km/s, v = 10 km/s, and w = 7 km/s (where u is directed toward the galactic center, v toward the direction of galactic rotation and w toward the northern galactic pole). km/s VLSRcom LSR rad. component "Radial component of the velocity of an object with respect to the LSR, at the same calculated position of the star, moving in the circular orbit defined by the galactic potential, vcr (in km/s)." km/s PVelrad Pecul. vel. rad. comp. Radial component of the peculiar velocity of the star, vpr = vLSR - vcr, in km/s km/s flag1 H II region flag "I" if the star is inside an H II region, "O" if it is outside --- H2Ident H II region ident. Identification of the H II region containing the star or of the H II region in the vicinity of the star. "MA" precedes the numbers of H II regions from the catalog of Marsalkova; "CYG" identifies stars found inside the Cygnus Nebula (S109 of Sharpless (1959). The number from Downes (1971) is listed in the notes for supernova remnants projected near the O star or H II region. --- D-H2 H II region distance Single-character code giving an approximate distance between a star and its associated H II region. The following codes are used: X phi < 0".5 Y 0".5 < phi < 1 deg Z phi > 1 deg pc GoyNum Goy (1973) number Number from the General Catalogue of O-Type Stars, Goy (1973) --- flag2 Note flag "*" if there is a note for this object in the second file --- rem Remark Miscellaneous remarks about the object. The following symbols appear: VVAR Velocity variable. The velocity range follows in parentheses. VVAR? Suspected velocity variable; little information available to determine variability VVAR(?) Suspected velocity variable; no single measurements given, variability stated without range SB ORB Single- or double-lined spectroscopic binary with known orbital elements. The magnitude difference follows in square brackets; the relative radial velocity is in parentheses. SB ORB? Spectroscopic binary with preliminary or provisional orbital elements. The magnitude difference follows in square brackets. SB Spectroscopic binary reported to have double lines. The magnitude difference follows in square brackets; the relative radial velocity is in parentheses. SB? Suspected double-line spectroscopic binary VB Visual binary corrected for contribution of bright, nearby component. The magnitude difference follows in brackets. EB Eclipsing binary. The depth of the primary eclipse in magnitudes follows in brackets. --- Notes CGO CGO number Number of the object to which this note refers --- rem Note Text of the note. When bytes 1-3 arc blank this field continues the note from the previous record. --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jun 22 UNKNOWN UNKNOWN The Catalogue of Galactic O Stars (CGO) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from E. Recillas-Cruz and J. F. Barral of the Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, in August 1982. The original tape consisted of two text files containing the main catalog data in the same format as the published catalog: the first file contained the data from the left-hand pages; the second file contained the data from the right-hand pages. A FORTRAN program was run to combine these two files into a single one. The spectral types were then converted from all upper-case to standard upper- and lower-case notation by means of an editor. ADC personnel keyed the notes from Cruz-Gonzalez et al. (1974) into a separate file. A FORTRAN program was run to check the validity of each field according to its data type and value. III_84B.xml Sixth Catalogue of Galactic Wolf-Rayet Stars 3085 III/85 Sixth Catalogue of Galactic Wolf-Rayet Stars Sixth Catalogue of Galactic Wolf-Rayet Stars K A van der Hucht P S Conti I Lundstrom B Stenholm Space Science Rev. 28 227 1981 1981SSRv...28..227V Stars, Wolf-Rayet Planetary nebulae This dataset consists of three files which reproduce data from three tables in the reference. The first file is a catalog of 159 Population I Galactic Wolf-Rayet Stars. The catalog includes a cross index between a running entry number, the best known or earliest catalog reference, HD, BD/CPD, CD, and LS. Each star also has a equatorial (1950.0) and galactic positions, precession to 2000.0, spectral type, binary information (if it applies), narrow-band v and b photometry, and reference codes for each of the previous data. The second file is a catalog of 45 Central Stars of Planetary Nebulae of Type [WR], [WR-Of], [O VI], [WC 10] and [WC 11]. The catalog contains a running entry number and identifications for the planetary nebula in which the star is located. Each star also has a equatorial (1950.0) and galactic positions, spectral type, visual magnitude, reference codes for each of the previous data, and an index for additional references which are in the third file.
159 Population I Galactic WR stars ID Identifier of entry. running number (1 - 158) --- suffix1 (only case is entry 29A) --- Cat1 A catalogue designation/number A catalog designation/number from one of the following references (full reference in Table 2 of this document): Designation: Number MR: numbers from Roberts (1962) NaSt: numbered after Nassau and Stephenson (1963) ST: numbers from Stephenson (1966) LS: numbers from Smith (1968a) MS: numbers from MacConnell and Sanduleak (1970) NS: numbered after Sanduleak (1971, 1976, 1979) BS: numbers from Stenholm (1975) StSa: numbered after Stephenson and Sanduleak (1977) BP: numbered after Petterson (1978) DA: numbered after Allen (1978, 1979). The two- or four-letter code for the paper, as given in the above list, is left-justified in the field. The number is right-justified in the rest of the field. The authors of the published catalogue add this comment: "The twelve WR stars discovered by Stephenson and Sanduleak (1971) are best known for their LSS number. Therefore we have refrained from creating additional StSa numbers for those stars." --- IdentA1 first additional identifier Alphabetical prefixes refer either to well-known catalogues to the following publications, for which full references are given in Table 2 of this document: AD: Arkhipova and Dokuchaeva (1971) AS: Merrill and Burwell (1950) BAC: Bordeaux Astrographic Chart BH: Hidayat (1962) CRL: Walker and Price (1975) He 2: Henize (1967) He 3: Henize (1976) HM: Herbig and Mendoza (1960) IC: Iriarte and Chavira (1956) Sand: Sanduleak (1971) TH: The (1961a, 1962a, b, 1963, 1965, 1966) Tr: The and Stokes (1970) Ve: Velghe (1957) WRA: Wray (1966) (only for stars without He 3-number) Other identifiers in this field may be Bayer names; or may be the Astrographic Catalogue (AC), the General Catalogue of Variable Stars (GCVS). GCVS Supplements, the New General Catalogue (NGC), the Index Catalogue (IC) or the Yale Bright Star Catalogue (HR). Note that the prefix "IC" is ambiguous. --- IdentA2 second additional identifier --- prefix1 star type "(" for companions to HD stars, "E" for HD Extension stars or blank --- HD Henry Draper (HD) numbers --- suffix2 "B)" for companions to HD stars --- DE1- sign of declination zone --- DEd1 absolute value of declination zone deg Sign1 decimal point standing for degree sign --- BD-CPD number of stars in the BD or CPD (Numbers) Number of stars within declination zone (bytes 42-44). Numbers from the Bonner Durchmusterung (BD) or Cape Photographic Durchmusterung (CPD). BD and the CPD overlap in the range -18 to -23 degrees. The published version of this catalogue does not make clear whether numbers in this range are BD or CPD numbers. --- DE2- sign of declination zone --- DEd2 absolute value of declination zone deg Sign2 decimal point standing for degree sign --- CD number of stars in the CD (Numbers) Number of stars within declination zone (bytes 52-54). Numbers from the Cordoba Durchmusterung (CD). --- SAO Numbers from SAO Star Catalogue --- prefix2 Henize Catalogues "2" if numbers from Henize (1967) or "3" if from Henize (1976). --- Dash (dash) --- Cat2 Numbers in the Henize catalogue Full references can be found in Table 2 below. --- LSnum The Luminous Stars (LS) numbers Numbers from the catalogues of Luminous Stars in the Northern Milky Way. The LS numbers of the last two stars in the published catalogue are grouped with a curly bracket. This is indicated in the machine-readable version by "*" in this byte of both corresponding entries (bytes 157 and 158). --- LS Identifier of specific LS catalogue Identifier of specific LS catalogue. Roman numeral, left-justified in field: I: numbers from Hardorp et al. (1959) II: numbers from Stock et al. (1960) III: numbers from Hardorp et al. (1964) IV: numbers from Nassau and Stephenson (1963) (see References in Table 2 below) --- DE3- sign of declination zone --- DEd3 absolute value of declination zone deg sign3 decimal point standing for degree sign --- StarNum number of stars in the Northern Milky Way Numbers of stars in the the catalogues of Luminous Stars in the Northern Milky Way. --- LSnum2 The LS numbers in the Southern Milky Way Number from Luminous Stars in the Southern Milky Way (Stephenson and Sanduleak, 1971 - full reference in Table 2 below). --- Cat3 Previous Catalogues of Wolf-Rayet stars Previous Catalogues of Wolf-Rayet stars in which this star appears, expressed as Roman numerals (for references, see Table 2 below): I: Campbell (1894) II: Fleming (1912) III: Payne (1930) IV: Roberts (1962) V: Smith (1968a) --- Correl1 Correlation with open cluster or association --- Correl2 Correlation with HII region Correlation with HII region, and "(r)" means "ring nebula". --- r_Correl1 References for Correl1 References for Correl1. A sequence of numbers in the range 1-143, separated by commas, pointing to entries in the reference dataset (see table9.dat and remarks.dat of this document). --- r_Correl2 References for Correl2 --- RAh Right ascension (equinox 1950) in hours h RAm minutes of right ascension min RAs seconds of right ascension s DE- sign of declination ("+" or "-") --- DEd degrees of declination (equinox 1950) deg DEm minutes of declination arcmin DEs second of declination arcsec PRAm Fifty year precession (to epoch 2000) min PRAs (Same as above) second of right ascension s PDE- Fifty year precession (to epoch 2000) --- PDEm precession in minutes of arc arcmin PDEs precession in seconds of arc arcsec GLON Galactic longitude (lII) deg GLATsign sign of bII ("+" or "-") --- GLAT Galactic latitude (bII) in degrees deg Sp Spectral type Spectral type according to the system described in Section 3 of the published catalogue. Table VII of the published catalogue summarizes the authors' spectral classification scheme and is reproduced as Table 3 of this document. Table XIV of the published catalogue gives the distribution of Wolf-Rayet stars by spectral subtype and is reproduced as Table 4 of this document. --- Period Period of orbit (unit = days). d Annotat Annotation to binary orbit. Annotation to binary orbit ":" refers to uncertainty in the period (bytes 241-248). "E" means "eclipsing", "SB1" means "optically invisible companion", and "SB2" means "WR+O system". --- flag1 "(" if V magnitude, "/" if mpg --- v(mag) value of magnitude v magnitude in narrow-band photometry in system of Smith (1968a, b - see Table 2 below), unless otherwise indicated. mag flag2 ":" indicates uncertainty of magnitude --- flag3 ")" if V magnitude, "/" if mpg --- flag4 "(" if B-V or estimated B-V --- b-v value of color index b-v color in narrow-band photometry in system of Smith (1968a, b - see Table 2 below), unless otherwise indicated. --- flag5 ":" indicates uncertainty of color index --- flag6 ")" if B-V or estimated B-V --- RefCoord References for equatorial coordinates See note on r_Correl1. --- r_Sp References for spectral type --- Reforbit References for binary orbit --- Refs References for v(mag) and b-v --- flag7 additional note information "*" if a note for this star is given in Table 1 of this document. --- Ident3 Identifier of star. Same as bytes 1-3. --- flag8 "A" for entry 29A only --- 45 Central (WR) Stars of Planetary Nebulae ID Running number of entry (1-45). --- Ident1 Identifier of central star of planetary nebula --- Ident2 Identifier of planetary nebula --- Ident3 Second identifier of planetary nebula --- GLON galactic longitude bin (degrees) Identifier of planetary nebula from Perek and Kohoutek (1967). See Table 2 below for reference deg GLATsign sign of galactic latitude zone --- GLAT absolute value of galactic latitude zone deg Num2 number within galactic coordinate bin --- RAh hours of right ascension (equinox 1950) Right ascension and Declination (epoch 1950). Equatorial coordinates are from Wackerling (1970), unless seconds of right ascension and arc seconds of declination are given, in which case they are from Barlow (1979, private communication) (see Table 2 below). h RAm minutes of right ascension (equinox 1950) min RAs seconds of right ascension (equinox 1950) s DE- sign of declination ("+" or "-") --- DEd degrees of declination (equinox 1950) deg DEm minutes of declination (equinox 1950) arcmin DEs seconds of declination (equinox 1950) arcsec Ref1 source - Perek and Kohoutek (1967) Spectral types as given in various sources. The full forms of the references to each of the following fields are given in Table 2 of this document. --- Ref2 source - Bohm (1968) --- Ref3 source - Aller (1968) --- Ref4 source - Smith and Aller (1969) --- Ref5 source - Aller (1976) --- Ref6 spectral type from some other source --- flag1 "(" may just mean left parenthesis The meaning of parenthesized magnitudes in the table9.dat was not stated by the authors. --- V V magnitude V magnitude described in bytes 129-136 is adopted from Aller (1976) or a source given in bytes 138-166. mag flag2 --- flag3 see byte 129 --- Ref7 Additional references Additional references. This field is a list of one- to three-digit numbers in the range 1-143 separated by commas. The numbers point to records in the reference file - see remarks.dat below. --- An index for additional references ID Running number of note or reference (1-143) Running number of note or reference (1-143). This number is referred to in the machine-readable versions of Tables VIII and IX of the catalogue, as described in table8.dat and table9.dat above. --- RefNote Reference or note Usually, a reference in bibliographical format. Each reference is complete in one record. This field may also contain a note on an individual datum, if in the published catalogue the note is referred to in a column also used for literature sources. --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Jul 13 The original ADC documentation by Robert S. Hill and Theresa A. Nagy (1982) was used to generate this ReadMe file. UNKNOWN UNKNOWN Tables 8 and 9 of the Wolf-Rayet Catalogue (see reference below) were keypunched at NASA/Goddard Space Flight Center from an early preprint, then were modified in accordance with revised preprints acquired from time to time thereafter. When the catalogue appeared in print, these datasets were modified to agree with the published version. The machine-readable version handles notes and references somewhat differently from the published version. In the published version, notes and references are pointed to sometimes with letters, sometimes with Arabic numerals, sometimes with Roman numerals. For the machine-readable version, a unified list of notes and references identified by Arabic numerals has been generated. The full bibliographic form of each reference is given. (Only those references pointed to by Tables 8 and 9 are included; those used only by the text and other tables of the catalogue have been omitted.) See table8.dat, table9.dat and remarks.dat of this document. Some information from the published version of the catalogue is reproduced in this document for the convenience of the user. In particular, notes on the individual stars (Table 1), references (Table 2), catalogue classification of WR spectra based on the Smith (1968a) system (Table 3) and distribution of Wolf-Rayet subclasses (Table 4) are given. Table 1. Notes on Individual Stars. No. 2: IUE spectra indicate He II 1640 and N V 1238 (A) emission spectrum only. Hence this is a Nitrogen class star. No. 3: Single star (Massey and Conti, 1981b, Paper V). No. 4: Strong Note A. No. 5: Note A (Aller, 1976). No. 6: Compact secondary according to Firmani et al. (1979) and McLean (1980) No. 8: Composite WN and WC spectrum. No. 11: Note A (Aller and Faulkner, 1964). No. 17: Note A. No. 26: Composite? WN component probably WN 5. C IV 5805 strong. C III-IV 4650 also present. No. 30: Note A. No. 33: Strong Note A. No. 41: Declination given by Stephenson and Sanduleak (1971) in error by almost 1.5'. No. 43: Not a single object (Walborn, 1973c). No. 46: Weak Note A (Sanduleak, 1968). No. 47: Most massive WR star known (Niemela, 1980). No. 48: Possible triple star, including 09.5 I member (Moffat and Seggewiss, 1977). Also visual double, with B3II star (Smith, 1955). No. 52: Weak Note A (Sanduleak, 1968). No. 57: Note A (Smith, 1955). No. 64: Appearing as No. 4 in the list by Stenholm (1975), but originally discovered by Stephenson and Sanduleak (1971). No. 72: Strong Note A (Sanduleak, 1971). No. 74: Classified from a slit spectrogram obtained by B. Pettersson. No. 85: Only 15" away from the G5Ia star HR 6392 (= HD 155603 = CD -39 deg 11212). Possible physical pair (Moffat and Fitzgerald, 1977, versus Lundstrom and Stenholm, 1979). No. 86: Single star (Massey, Conti and Niemela, 1981, Paper VII). No. 88: Star discovered by The (1961a, b) and listed as MR 70 by Roberts (1962). Erroneously Smith (1968a, b) studied a star 5 deg North of MR70, as noted by Stephenson and Sanduleak (1971), Johnson (1973b) and Sanduleak (1974). No. 90: Note A (Smith, 1955). No. 97: Strong absorption spectrum. H a emission and the absence of a Pickering emission spectrum is noteworthy. No. 98: Composite spectrum. Might be a single star. No. 102: Classified from the spectrogram obtained by Freeman et al. (1968). No. 103: Compact companion? (Isserstedt and Moffat, 1981). No. 105: This new WR star lies not far from, and may have been confused in the past with, No. 104. No. 107: Classified from a spectrogram obtained by Alien (1978). No. 108: Star discovered by Cannon and Mayall (1938) and listed as LS 14 by Smith (1968a), but her declination is 8' off, as noted by Stephenson and Sanduleak (1971) and MacConnell and Bidelmann (1976). No. 111: Note A (Bappu, 1973). No. 116: Independently discovered by Dolidze (1959) and Stephenson (1966). No. 122: Discovered by Nassau and Stephenson (1963). Erroneously identified as a planetary nebula by Stephenson (1966; Stephenson, 1979, private communication). No. 123: Single star (Massey and Conti, 1980a, Paper II). No. 135: Weak Note A (Underhill, 1959; Sanduleak, 1968). No. 136: Compact component? (Moffat and Seggewiss, 1980a). No. 137: Single star (Massey, Conti and Niemela, 1981, Paper VII). No. 138: Probably single star (Massey, 1980a, Paper I). No. 140: Single star (Conti and Roussel-Dupree, 1981). No. 141: OB companion dubious, N IV composite, ... No. 142: Strong Note A (Sanduleak, 1971). No. 143: No companion. No. 145: Composite WN + WC spectrum, not classifiable. No. 148: Compact companion? Moffat's runaway (Moffat and Seggewiss, 1980b). No. 154: Note A. No. 156: Note A. No. 157: Visual binary (Wilson, 1940; Crampton, 1975). Separation 1". Brighter companion is a B star. No. 29a: Discovered by MacConnell and Sanduleak (1970). Stenholm (1975) failed to detect any emission lines in this rather bright star, and it was therefore deleted from our catalogue. However, a slit spectrogram recently obtained by PSC confirms the WR nature of this star. Including the star as its proper place would have delayed the publication of the Catalogue. Note A: O VI 3811 A, 3834 A emission. Table 2. References for This Document Allen, D. A., 1978, Monthly Notices Roy. Astron. Soc. 184, 601. Allen, D. A., 1979, Observatory, 99, 83. Aller, L. H., 1968. in D. R. Osterbrock and C. R. O'Dell (eds.), 'Planetary Nebulae', IAU Symp. 34, 340. Aller, L. H., 1976, Mem. Soc. Roy. des Sci. de Liege, 6e Ser. 9, 271. Arkhipova, V. P. and Dokuchaeva, O. D., 1971, Astron. Zh. 48, 752 (=1972, Soviet Astron.-AJ 15, 593). Bohm, K. H., 1968, in D. R. Osterbrock and C. R. O'Dell (eds.), 'Planetary Nebulae', IAU Symp. 34, 312. Campbell, W. W., 1894, Astron. Astrophys. 13, 448. Fleming, W. P., 1912, Harvard College Obs. Ann. 56, 165. Hardorp, J., Rohlfs, K., Slettebak, A. and Stock, J., 1959, Luminous Stars in the Northern Milky Way, I, Hamburg-Bergedorf. Hardorp, J., Theile, I. and Voigt, H. H., 1964, Luminous Stars in the Northern Milky Way, III, Hamburg-Bergendorf. Henize, K. G., 1967, (He2-Catalog), Astrophys. J. Suppl. 14, 125. Henize, K. G., 1976, (He3-Catalog), Astrophys. J. Suppl. 30, 491. Herbig, G. H. and Mendoza, E. E., 1960, bol. Obs. Tonantzintla y Tachbaya 2 (no. 19), 21. Hidayat, B., 1962, Contr. Bosscha Obs., No. 16. Iriarte, B. and Chavira, E., 1956, Bol. Obs. Tonantzintla Y Tacubava 2, (No. 14), 31. MacConnell, D. J. and Sanduleak, N., 1970., Publ. Astron. Soc. Pacific 82, 80. Merrill, P. W. and Burwell, C. G., 1950, Astrophys. J. 112, 72. Nassau, J. J. and Stephenson, C. B., 1963, Luminous Stars in the Northern Milky Way, IV, Hamburg-Bergedorf. Payne, C. H., 1930, The Stars of High Luminosity, Harvard Obs. Monographs, No. 3, p.l9 Perek, L. and Kohoutek, L., 1967, Catalogue of Galactic Planetary Nebulae, Prague, Czechoslovakian Acad. of Sci. Petterson, B., 1978, private communication to Lundstrom and Stenholm (1979) Roberts, M. S., 1962, Astron. J. 67, 79. Sanduleak, N., 1971, Astrophys. J. (Letters) 164, L71. Smith, L. F., 1968a, Monthly Notices Roy. Astron. Soc. 138, 109. Smith, L. F. and Aller, L. H., 1969, Astrophys. J. 157, 1245. Stenholm, B., 1975, Astron. Astrophys. 39, 307. Stephenson, C. B., Astron. J. 71, 477. Stephenson, C. B., 1979, private communication. Stephenson, C. B. and Sanduleak, N., 1971, 'Luminous Stars in the Southern Milky Way', PubL Warner and Swasey Obs. 1, No.1 . Stephenson, C. B. and Sanduleak, N., 1977, Publ. Warner and Swasey Obs. 2, No. 4. Stock, J., Nassau, J. J. and Stephenson, C. B., 1960, Luminous Stars in the Northern Milky Way, II, Hamburg-Bergedorf. The, P. S., 1961a, Contr. Bosscha Obs., No. 10. The, P. S., 1962a, Contr. Bosscha Obs., No. 14. The, P. S., 1962b, Contr. Bosscha Obs., No. 17. The, P. S., 1963, Observatory 83, 83 (Contr. Bosscha Obs., No. 20). The, P. S., 1965, Observatory 85, 122 (Contr. Bosscha Obs., No. 31). The, P. S., 1966, Contr. Bosscha Obs., No. 35. The, P. S. and Stokes, N., 1970, Astron. Astrophys. 5, 298. Velghe, A. G., 1957, Astrophys. J. 126, 302. Wackerling, L. R., 1970, Mem. Roy. Astron. Soc. 73, 159. Walker, R. G. and Price, S. D., 1975, AFCRL Infrared Sky Survey, 1, Air Force Report AFCRL-TR-75-0373. Wray, J. D., 1966, Dissertation, Northwestern University, Evanston, Illinois, Table 15 Table 3. Catalogue Classification of WR Spectra Based on the Smith (1968a) System. WN types Nitrogen ions Other criteria WN 9 N III present, N IV weak or absent He I, lower Balmer series P Cyg WN 8 NIII >> NIV He I strong P Cyg, N III 4640 < He II 4686 WN 7 N III > N IV He I weak P Cyg, N III 4640 < He II 4686 WN 6 N III =~ N IV, N V present but weak WN 5 N III =~ N IV =~ N V WN 4.5 N IV > N V, N III weak or absent WN 4 N IV =~ N V, N III weak or absent WN 3 N IV << N V, N III weak or absent WN 2 N V weak or absent Strong He II WC types Carbon ions Carbon, oxygen ions Other 5696 C III/5805 C IV 5696 C III/5592 O V Criteria WC 9 C III > C IV O V weak or absent C II present WC 8.5 C IIl > C IV O V weak or absent C II not present WC 8 C III =~ C IV O V weak or absent WC 7 C III < C IV C III >> O V WC 6 C III << C IV C III > O V WC 5 C III << C IV C III < O V WC 4 C IV strong, O V moderate C III weak or absent Table 4. Distribution of Wolf-Rayet Sub-Classes (galactic). WR subclass Single Double --------------------- ------------- Single Single + abs SB 2 SB 1 WN 2 1 WN 3 3 1 WN 4 9 4 WN 4.5 5 1 WN 5 5 1 1 1 WN 6 14 2 2 WN 7 10 3 1 2 WN 8 10 WN 9 1 WN 1 2 ------------------------------------------------------ Subtotal WN 59 7 9 5 ------------------------------------------------------ WC 4 6 WC 5 12 1 WC 6 11 3 1 WC 7 5 3 2 WC 8 5 1 2 WC 8.5 6 WC 9 12 WC 1 ------------------------------------------------------- Subtotal WC 58 8 5 ------------------------------------------------------- WN+WC 2 1 WR 4 1 ------------------------------------------------------- ------------------------------------------------------- Grand Total 123 16 14 6 III_85.xml Catalog of Far-Ultraviolet Objective-Prism Spectrophotometry: Skylab Experiment S-019, Ultraviolet Stellar Astronomy 3086 III/86 SKYLAB S-019 Far-UV Objective-Prism Spectrophot Catalog of Far-Ultraviolet Objective-Prism Spectrophotometry: Skylab Experiment S-019, Ultraviolet Stellar Astronomy K G Henize J D Wray S B Parsons G F Benedict NASA Ref. Publ. 1031 ??? ??? 1979 1979cfuo.book.....H Spectrophotometry Spectra, ultraviolet The catalog contains arrays of ultraviolet flux measurements at wavelengths of 1300-4200 angstroms. The data were obtained with an objective-prism telescope (an f/3 Ritchey-Chretien system with a 15-cm aperture and a calcium fluoride-lithium fluoride focal-plane corrector). The spectra were digitized with a PDS 1010A microdensitometer, and each spectrum was scanned in a series of 30-micron strips. This catalogue contains data on 494 stars. The data on each star are quite complex and include the adopted fluxes, exposure data, intermediate-band magnitudes, and cross identifications to the numbering system of The Henry Draper Catalogue.
ASCII catalog version HD Henry Draper Catalogue (HD) number Henry Draper Catalogue (HD) number of the star. Table 4-1 below is a list of all the stars in this file. --- alt Alternative name of the star. Alternative name of the star. When no alternative name is given, these bytes are the same as bytes 1-10 --- Edata Exposure data, encoded. Exposure data. These data are contained in five fields or 37 bytes apiece. For most stars, fewer than five exposures were used. In this case, the exposure data fields are filled from left to right, and the fields not used contain blanks. 21-57 A37 Edata1 - First exposure data 58-94 A37 Edata2 - Second exposure data or blank. 95-131 A37 Edata3 - Third exposure data or blank. 132-168 A37 Edata4 - Fourth exposure data or blank. 169-205 A37 Edata5 - Fifth exposure data or blank. The exposure field format in terms of byte offsets is as follows: +0 to +6 Plate number. Information on each frame taken throughout the experiment can be found in the second file of this catalogue by keying on this plate number. See Byte-by-byte Description for exposure.dat below, bytes 1-7. +8 to +10 Exposure time in seconds. If no precise time was available (because of gaps in the observing log), a reasonable default value is used. +11 ':' if a default value is used for the exposure time in offsets +8 to +10, otherwise blank. +13 to +17 X position of the star on the plate in millimeters (mm) +19 to +23 Y position of the star on the plate in millimeters (mm) "The plate position ... refers to the position of the optical head of the spectrum with respect to the field center, measured at the original plate scale. Coordinates are defined such that, with the frame oriented (with) shorter wavelengths toward the left, X increases toward the left and Y increases toward the bottom. The dimensions of the 4 by 5 degrees field are 32 mm by 40 mm on this scale." NOTE: At this writing, prints of the S-019 frames can be obtained from the National Space Science Data Center as described in the Remarks and Modifications below. +25 to +26 Number of microdensitometer scans of the stellar spectrum. Each scan is a longitudinal strip 30 microns (um) wide; thus multiplying by 30 um gives the approximate width of the spectrum. The portions that overlap with other stars are not included. +28 to +30 The weight of the spectrum. "The assigned weight ... for each spectrum depends partly on the measurable width and partly on the presumed quality of the reduction. The (Skylab mission) SL4 spectra normally receive a weight of 0.6 or 0.7, instead of 0.9 or 1.0, because the emulsion batch used was grainier and had poorer photometric properties than the batch used on SL2 and SL3." +32 to +35 Scale value, which is "the relative scaling of the flux values for maximum agreement prior to averaging the different exposures. It also was used to make an approximate adjustment when less than the full width of the spectrum could be scanned." --- Com1 First part of comment notation. Can be "(" "<", or blank. See bytes 211-213. The comment notation, which describes different cases and methods for the flux adjustment calculation, is in bytes 206 and 211-213 in the same form as in the published catalogue. A full explanation of this notation is given in the Remarks and Modifications below. --- FAfactor Flux adjustment factor r for the star Flux adjustment factor r for the star, defined by this formula: (absolute flux)= (S-019 flux)*r "The absolute flux levels for most stars were compared with other satellite measurements or with predicted fluxes to assess the accuracy of the calibration and to provide the user with adjustment factors." (the flux is measured in units of ergs cm-2 sec-1 A-1, see below.) --- Com2 The second part of the comment notation, or else blank. The notations in this field consist of one or more of ")", ">", ":", "::", and "+-". See also byte 206. --- Flux Flux data, encoded. Each flux data is in a 10-byte field which contains all the information in the published catalogue except the wavelength. The wavelength is determined by the bytes in which the field appears. Note that floating-point (F format) data have implicit decimal points. The correspondence between wavelength and byte is determined by the following table, in which BW is the bandwidth, MIN is the minimum of the possible wavelengths in angstroms (A) for that bandwidth, MAX is the maximum of the possible wavelengths in A for that bandwidth, and BASE is the first byte of the ten-byte field corresponding to MIN. The values MAX are redundant for determining the correspondence, but are given for clarity. COUNT is the greatest number of fluxes that can be given for each bandwidth; i.e., the number of ten-byte fields in that part of the record. Table 2-1(a). Constants for Determining Wavelength and Bandwidth from Byte Position. BASE BW(A) (BYTE) MIN(A) MAX(A) COUNT 2 214 1310 1828 260 5 2814 1800 2320 105 10 3864 2300 3040 75 20 4614 3000 4180 60 The wavelengths appear in ascending order starting at the given base bytes, each successive 10-byte field representing an increment by the bandwidth. Thus, the following formula converts a byte number (BYTNUM) to the corresponding wavelength (Lambda): Lambda = ((BYTNUM-BASE)/10) *BW + MIN The following is a description of the flux field format in terms of byte offsets: +0 (A1) Comment character--either a blank or one of the following: U - underexposure; the average intensity only a little above the background fog E - extreme exposure; the average intensity not far from saturation L - overlapping star D - plate defect +1 to +3 (I3) Digits (D) of flux measurement, as in the formula below. +4 (I1) Order-of-magnitude code (C) of flux measurement, as in the below formula. Note on Flux measurement. Approximately the absolute flux incident at the earth, averaged over the range Lambda - BW/2 to Lambda + BW/2, where BW has one of the values in Table 2-1(a), and where Lambda is related to the absolute position of the field in the record by the formula given after Table 2-1(a). This value is given in modified exponential notation, with two values D (digits) and C (order-of-magnitude code), such that flux=D * 10**(-C-8) ergs cm-2 sec-1 A-1 The flux is a weighted average of the data points for the wavelength from all the exposures. Each individual weight is a function of the slope of the characteristic curve of the emulsion at the density of the particular wavelength (which can vary from exposure to exposure), with the straight-line portion weighted at 1.0. There are eight dummy data points in the catalogue, and in the published version these are represented by flux values on the order of 10**(-24). These instances are listed in Table 4-2 of this document and are represented by all blank flux fields in the machine-readable version. +5 to +6 Total weight of the wavelength. This number is calculated from weights contributed by the individual spectra. It refers mainly to the accuracy of the absolute fluxes, rather than to spectral details. It also reflects the general reliability of the data in the region, as indicated by the comment character at offset +0. The weights of the component spectra are described under offsets +1 to +4. +7 to +9 Standard deviation, according to the following formula, as a percentage of the average flux given at offsets +1 to +4: Sig = the standard deviation N = the number of spectra averaged Wi = the weight of an individual spectrum as described under offsets +1 to +4 Si = the scale factor for the exposure, given in offsets +22 to +25 of each exposure- data field (see bytes 21-205 above) Fi = the flux in an individual spectrum F = the average flux as given in offsets +1 to +4 The standard deviations "reflect both grain noise and the effects of differences in slope among the derived energy distributions." A long series of zero standard deviations means that only one exposure was used in that region. --- IBmag Intermediate-band magnitudes These are computed over comparatively wide wavelength intervals and are related to the fluxes by MAG =-2.5*log F- 21.10 where F is the average flux over the interval. The constant, corresponding to 3.64 x 10**(-9) ergs cm-2 sec-1 A-1 was adopted in accordance with Nandy et al. (l976), "in order to put the magnitudes on the same energy scale as visual V magnitudes. The value of F is a straight average (rectangular passband), except for the 360 nanometer (nm) band, where a Johnson U filter function is used (Mathews and Sandage 1963). Based on the absolute calibration of U magnitudes (Johnson 1966), approximately 0.20 magnitude should be subtracted to put the ground-based U values on the same energy scale." In this magnitude system, the width of each passband on the film is a constant 360 um. The intermediate-band magnitudes are in ten-byte fields of the same form as the flux fields above, with differences which will be explained below. The following table shows the starting byte of each intermediate-band magnitude field: Table 2-1b. Intermediate-Width Passbands FIRST CENTRAL RANGE BYTE Lambda(nm) (A) FEATURES 5214 135 1347 - 1364 Continuum. 5224 139 1385 - 1405 Si IV lines. 5234 148 1465 - 1495 Continuum. 5244 154 1521 - 1560 C IV plus Fe II plus Si II lines. 5254 161 1587 - 1636 Temperature- and gravity-sensitive blends. 5264 166 1636 - 1693 Continuum; blends in hotter stars. 5274 172 1693 - 1760 Gravity-sensitive blend. 5284 181 1770 - 1853 Continuum 5294 192 1870 - 1975 Gravity-sensitive depression (Fe III). 5304 204 1975 - 2110 Continuum. 5314 219 2110 - 2290 Continuum; interstellar extinction 5324 245 2320 - 2600 Continuum; Fe II in cooler stars. 5334 280 2600 - 3070 Continuum; Mg II in cooler stars. 5344 360 3070 - 4100 Continuum; approximate Johnson U magnitude Following is a description of the field format of the intermediate band magnitudes according to byte offsets. +0 Comment character. See offset +0 under bytes 214-5213 above. +1 to +3 Magnitude as described above, with a decimal point implicit between offsets +1 and +2. +5 to +6 Total weight for the passband. See offsets +5 to +6 under bytes 214-5213 above. +7 to +9 Standard deviation. See offsets +7 to +9 under bytes 214-5213 above. This standard deviation is to be interpreted slightly differently from those in bytes 214-5213: this value is "computed from the differences among the magnitudes from separate exposures, hence the grain noise component is eliminated." --- Exposure Data Fnum Frame number Frame number. Each exposure has 8 unique identifier which is referred to in the data file (see data.dat, bytes 21-205). Each exposure number, also called a frame number, consists of a mission number (SL2, SL3, or SL4), and an integer exposure sequence number. --- flag1 "(" if the field center is uncertain --- RAh Right ascension (1950) of field center Field center. "The celestial orientation of Skylab was often uncertain by 1 degree or more, so all field centers were determined with the Becvar atlases (Becvar 1962, 1964). On the prism exposures, the highly compressed optical end (head) of the spectrum, ending near 5000 A, was used for positional reference." This field is blank if the frame was for calibration or was unusable because of defects, fogging, bad exposure, etc. h flag2 (colon). --- RAm Minutes of right ascension min DEdeg Declination (1950) of field center deg flag3 ")" if the field center is uncertain --- Field Field designation. Field designation. Five character designation for internal use by the S-019 investigators. --- Year Calendar year of exposure. yr Month Month of exposure --- Day Day of exposure d UTd Universal time of year following Jan. 0.0. Universal Time (UT) for the start of each exposure. Bytes 37-48 are blank for calibration exposures. "Start and end times could be determined to the nearest second from verbal 'marks' given by the astronaut and recorded on two-track tape, the second track containing a time signal. (Approximately 25 percent of) this information is lost, in which case the start time is given to the nearest minute and should be within 2 minutes of the actual start of the observation." d flag4 (colon) --- UTh UT of exposure, hours h flag5 (colon) --- UTm UT of exposure, minutes min flag6 or blank if the exact start time was lost --- UTs UT of exposure, seconds s CanNum Serial number of the film canister. --- Tangle Tilt angle Tilt angle, which refers to the Articulated Mirror System (Henize et al. 1979). At 0 degree tilt, the line of sight makes a 30 degree angle with the spacecraft wall. Bytes 56-77 are blank for calibration exposures. deg PA Position angle Position angle, defining the orientation of north on the frame. With the print oriented so that shorter wavelengths are toward the left, the zero point of position angle is toward the top. The angle is measured clockwise in degrees. deg Etime The planned, nominal exposure time in seconds s Com Blank, or comment character Blank, or the following comment character: U = unwidened spectra N = no prism, direct photograph --- flag7 "(" if the actual exposure t is uncertain --- Mtime Actual measured exposure time Actual measured exposure time when determinable from the voice marks (see bytes 37-48). s flag8 ")" if the actual exposure t is uncertain --- rem Remarks. Two exposures have extremely long remarks which are not included in the machine-readable version and are as follows: RECORD NO. FRAME REMARK 377 SL4-050 Started before comet rise, total 253 sec 417 SL4-090 Resembles very short U expo. According to transcript, it may have been terminated after 10 sec., <- 219. The following are the explanations given by Heinze et al. (1979) for abbreviations appearing in the remarks: REMARK MEANING ATM.EXT Indicates spectra are affected by atmospheric extinction. END: Gives end time of exposure to nearest second when known, if start time was not recorded. (FOGGED) Indicates plate has narrow streak of fog, or general fog greater than normal. FOGGED Indicates plate has heavy fog, but images may be usable. HIFOG Indicates plate has severe fog, images not usable. NO IMD Indicates the spectra are trailed due to failure to inhibit momentum dumping. <- Indicates field was renumbered from the pad designation. -> Indicates this field now shared between two adjacent fields. --- HD358.fit FITS table of ALF AND HD432.fit FITS table of BET CAS HD593.fit FITS table of HD593 HD1337.fit FITS table of AOCAS HD1976.fit FITS table of HR91 HD2054.fit FITS table of HR96 HD2772.fit FITS table of LAM CAS HD2905.fit FITS table of KAP CAS HD3240.fit FITS table of HR144 HD3360.fit FITS table of ZET CAS HD4142.fit FITS table of HR189 HD4180.fit FITS table of OMI CAS HD5394.fit FITS table of GAM CAS HD5408.fit FITS table of HR266 HD10144.fit FITS table of ALF ERI HD10516.fit FITS table of PHI PER HD16349.fit FITS table of HD16349 HD18925.fit FITS table of GAM PER HD19268.fit FITS table of HR930 HD19356.fit FITS table of BET PER HD20191.fit FITS table of HD20191 HD20283.fit FITS table of HR979 HD20677.fit FITS table of 32PER HD20809.fit FITS table of HR1011 HD20902.fit FITS table of ALF PER HD21364.fit FITS table of XITAU HD21428.fit FITS table of 34PER HD21551.fit FITS table of HR1051 HD21686.fit FITS table of 4 TAU HD21699.fit FITS table of HR1063 HD21856.fit FITS table of HR1074 HD21933.fit FITS table of 6 TAU HD22192.fit FITS table of PSI PER HD22780.fit FITS table of HR1113 HD22928.fit FITS table of DEL PER HD22951.fit FITS table of 40PER HD23193.fit FITS table of HR1133 HD23302.fit FITS table of 17TAU HD23630.fit FITS table of ETA TAU HD23753.fit FITS table of HR1172 HD23848.fit FITS table of 42PER HD23985.fit FITS table of HR1188 HD24398.fit FITS table of ZET PER HD24504.fit FITS table of HR1207 HD24534.fit FITS table of X PER HD24640.fit FITS table of HR1215 HD24912.fit FITS table of XIPER HD25940.fit FITS table of 48PER HD27045.fit FITS table of OMG TAU HD27295.fit FITS table of 53TAU HD27309.fit FITS table of 56TAU HD27396.fit FITS table of 53PER HD27934.fit FITS table of KAP TAU HD27946.fit FITS table of 67TAU HD28024.fit FITS table of UPS TAU HD28319.fit FITS table of THT-2 TAU HD28546.fit FITS table of 81TAU HD28556.fit FITS table of 83TAU HD28879.fit FITS table of HD28879 HD28910.fit FITS table of RHO TAU HD29479.fit FITS table of SIG-1 TAU HD29488.fit FITS table of SIG-2 TAU HD31512.fit FITS table of 62ERI HD32068.fit FITS table of ZET AUR HD32249.fit FITS table of PSI ERI HD32630.fit FITS table of ETA AUR HD32964.fit FITS table of 66ERI HD33111.fit FITS table of BET ERI HD33328.fit FITS table of LAM ERI HD33904.fit FITS table of MULEP HD33948.fit FITS table of HR1704 HD34029.fit FITS table of ALF AUR HD34085.fit FITS table of BET ORI HD34503.fit FITS table of TAU ORI HD34816.fit FITS table of LAM LEP HD35007.fit FITS table of HR1764 HD35039.fit FITS table of 22ORI HD35149.fit FITS table of 23ORI HD35299.fit FITS table of HR1781 HD35337.fit FITS table of 8 LEP HD35439.fit FITS table of 25ORI HD35468.fit FITS table of GAM ORI HD35575.fit FITS table of HD35575 HD35588.fit FITS table of HR1803 HD35708.fit FITS table of 114 TAU HD35715.fit FITS table of PSI ORI HD35912.fit FITS table of HR1820 HD36267.fit FITS table of 32ORI HD36285.fit FITS table of HR1840 HD36351.fit FITS table of 33ORI HD36430.fit FITS table of HR1848 HD36486A.fit FITS table of DEL ORI HD36486.fit FITS table of DEL ORI HD36512.fit FITS table of UPS ORI HD36591.fit FITS table of HR1861 HD36695.fit FITS table of VVORI HD36779.fit FITS table of HR1873 HD36822.fit FITS table of PHI-1 ORI HD36827.fit FITS table of HD36827 HD36861.fit FITS table of LAM ORI HD36895.fit FITS table of HD36895 HD36960.fit FITS table of HR1887+86 HD37041.fit FITS table of THT-2 ORI HD37043.fit FITS table of IOT ORI HD37128.fit FITS table of EPS ORI HD37150.fit FITS table of HR1906 HD37202.fit FITS table of ZET TAU HD37209.fit FITS table of HR1911 HD37269.fit FITS table of 26AUR HD37303.fit FITS table of HR1918 HD37468.fit FITS table of SIG ORI HD37481.fit FITS table of HR1933 HD37490.fit FITS table of OMG ORI HD37507.fit FITS table of 49ORI HD37742.fit FITS table of ZET ORI HD37744.fit FITS table of HR1950 HD37756.fit FITS table of HR1952 HD39985.fit FITS table of HR2075 HD42087.fit FITS table of 3 GEM HD42216.fit FITS table of HD42216 HD42933.fit FITS table of DEL PIC HD45057.fit FITS table of HD45057 HD45348.fit FITS table of ALF CAR HD45789.fit FITS table of HD45789 HD45995.fit FITS table of HR2370 HD46300.fit FITS table of 13MON HD46885.fit FITS table of HR2413 HD46966.fit FITS table of HD46966 HD47129.fit FITS table of HR2422 HD47417.fit FITS table of HD47417 HD47839.fit FITS table of 15S MON HD48099.fit FITS table of HR2467 HD48917.fit FITS table of 10CMA HD49961.fit FITS table of HD49961 HD50013.fit FITS table of KAP CMA HD50123.fit FITS table of HR2545 HD51411.fit FITS table of HR2598 HD52140.fit FITS table of HR2621 HD52670.fit FITS table of HR2640 HD53138.fit FITS table of OMI-2 CMA HD53344.fit FITS table of HD53344 HD54605.fit FITS table of DEL CMA HD54893.fit FITS table of HR2702 HD54912.fit FITS table of HR2704 HD55522.fit FITS table of 26CMA HD55857.fit FITS table of HR2734 HD55879.fit FITS table of HR2739 HD55958.fit FITS table of HR2741 HD55985.fit FITS table of HR2743 HD56014.fit FITS table of 27CMA HD56094.fit FITS table of HD56094 HD56139.fit FITS table of OMG CMA HD56342.fit FITS table of HR2756 HD56455.fit FITS table of HR2761 HD56554.fit FITS table of HD56554 HD56779.fit FITS table of HR2770 HD56876.fit FITS table of HR2774 HD57060.fit FITS table of 29UW CMA HD57061.fit FITS table of TAU CMA HD57150.fit FITS table of HR2787 HD57193.fit FITS table of HD57193 HD57219.fit FITS table of HR2790 HD57593.fit FITS table of HR2800 HD58011.fit FITS table of HD58011 HD58260.fit FITS table of HD58260 HD58286.fit FITS table of HR2823 HD58325.fit FITS table of HR2824 HD58350.fit FITS table of ETA CMA HD58420.fit FITS table of HR2829 HD58612.fit FITS table of HR2841 HD58978.fit FITS table of HR2855 HD59026.fit FITS table of HR2856 HD59136.fit FITS table of HR2860 HD59499.fit FITS table of HR2870+71 HD59527.fit FITS table of HD59527 HD59550.fit FITS table of HR2873 HD59864.fit FITS table of HD59864 HD60098.fit FITS table of HR2885 HD60168.fit FITS table of HR2889 HD60312.fit FITS table of HR2895 HD60344.fit FITS table of HD60344 HD60606.fit FITS table of HR2911 HD61071.fit FITS table of HD61071 HD61330.fit FITS table of HR2937 HD61429.fit FITS table of HR2944 HD62315.fit FITS table of HD62315 HD62623.fit FITS table of 3 PUP HD62747.fit FITS table of HR3004 HD63308.fit FITS table of HR3025 HD63425.fit FITS table of HD63425 HD63462.fit FITS table of OMI PUP HD63465.fit FITS table of HR3035 HD63868.fit FITS table of HD63868 HD64365.fit FITS table of HR3078 HD64440.fit FITS table of HR3080 HD65315.fit FITS table of HR3107 HD66624.fit FITS table of HR3162 HD66811.fit FITS table of ZET PUP HD68092.fit FITS table of HD68092 HD68161.fit FITS table of HR3203 HD68273.fit FITS table of GAM VEL HD68324.fit FITS table of HR3213 HD68657.fit FITS table of HR3227 HD68761.fit FITS table of HD68761 HD68895.fit FITS table of HR3234 HD68980.fit FITS table of HR3237 HD69106.fit FITS table of HD69106 HD69144.fit FITS table of HR3244 HD69168.fit FITS table of HD69168 HD69302.fit FITS table of HR3250 HD69404.fit FITS table of HD69404 HD69973.fit FITS table of HD69973 HD70309.fit FITS table of HD70309 HD70556.fit FITS table of HR3283 HD70930.fit FITS table of HR3294 HD71935.fit FITS table of HR3350 HD72108.fit FITS table of HR3358 HD72232.fit FITS table of HR3363 HD72737.fit FITS table of HR3386 HD73105.fit FITS table of HD73105 HD74071.fit FITS table of HR3440 HD74146.fit FITS table of HR3442 HD74195.fit FITS table of OMI VEL HD74319.fit FITS table of HD74319 HD74371.fit FITS table of HR3456 HD74956.fit FITS table of DEL VEL HD75241.fit FITS table of HD75241 HD75821.fit FITS table of HR3527 HD76004.fit FITS table of HD76004 HD76538.fit FITS table of HR3560 HD76566.fit FITS table of HR3562 HD76728.fit FITS table of HR3571 HD77002.fit FITS table of HR3582 HD77320.fit FITS table of HR3593 HD77475.fit FITS table of HR3600 HD78616.fit FITS table of HD78616 HD79186.fit FITS table of HR3654 HD79351.fit FITS table of A.CAR HD79416.fit FITS table of HR3661 HD79447.fit FITS table of HR3663 HD79694.fit FITS table of HR3672 HD79735.fit FITS table of HR3674 HD80404.fit FITS table of IOT CAR HD83944.fit FITS table of HR3856 HD83979.fit FITS table of ZET CHA HD84228.fit FITS table of HR3868 HD84809.fit FITS table of HR3883 HD85871.fit FITS table of HR3920 HD86440.fit FITS table of PHI VEL HD87737.fit FITS table of ETA LEO HD87901.fit FITS table of ALF LEO HD90853.fit FITS table of HR4114 HD91316.fit FITS table of RHO LEO HD91465.fit FITS table of PPCAR HD92664.fit FITS table of HR4185 HD92740.fit FITS table of HR4188 HD93030.fit FITS table of THT CAR HD93194.fit FITS table of HR4205 HD93845.fit FITS table of DEL-2 CHA HD97583.fit FITS table of HR4355 HD100841.fit FITS table of LAM CEN HD101379.fit FITS table of HR4492 HD102249.fit FITS table of LAM MUS HD102647.fit FITS table of BET LEO HD103079.fit FITS table of HR4549 HD106983.fit FITS table of ZET CRU HD108248.fit FITS table of ALF CRU HD110335.fit FITS table of HR4823 HD112078.fit FITS table of LAM CRU HD113904.fit FITS table of THT MUS HD114529.fit FITS table of HR4975 HD114911.fit FITS table of ETA MUS HD115846.fit FITS table of HD115846 HD116658.fit FITS table of ALF VIR HD117651.fit FITS table of HR5093 HD120640.fit FITS table of HR5206 HD120991.fit FITS table of HR5223 HD121483.fit FITS table of HD121483 HD121790.fit FITS table of UPS-1 CEN HD122451.fit FITS table of BET CEN HD124367.fit FITS table of HR5316 HD125238.fit FITS table of IOT LUP HD125288.fit FITS table of HR5358 HD125721.fit FITS table of HR5375 HD125823.fit FITS table of HR5378 HD126341.fit FITS table of TAU-1 LUP HD126759.fit FITS table of HD126759 HD126983.fit FITS table of HR5413 HD127381.fit FITS table of SIG LUP HD127971.fit FITS table of HR5439 HD127972.fit FITS table of ETA CEN HD128345.fit FITS table of RHO LUP HD128620.fit FITS table of ALF CEN HD128974.fit FITS table of HR5466 HD129056.fit FITS table of ALF LUP HD129092.fit FITS table of HD129092 HD129116.fit FITS table of HR5471 HD129422.fit FITS table of HR5482 HD129929.fit FITS table of HD129929 HD130559.fit FITS table of MULIB HD130701.fit FITS table of AXCIR HD130807.fit FITS table of OMI LUP HD130819.fit FITS table of ALF-1 LIB HD130841.fit FITS table of ALF-2 LIB HD131120.fit FITS table of HR5543 HD131492.fit FITS table of THT CIR HD132058.fit FITS table of BET LUP HD132200.fit FITS table of KAP CEN HD133738.fit FITS table of HD133738 HD133955.fit FITS table of LAM LUP HD134657.fit FITS table of HD134657 HD134687.fit FITS table of HR5651 HD135160.fit FITS table of HR5661 HD135240.fit FITS table of DEL CIR HD135591.fit FITS table of HR5680 HD135734.fit FITS table of MULUP HD135917.fit FITS table of HD135917 HD136415.fit FITS table of GAM CIR HD136504.fit FITS table of EPS LUP HD138690.fit FITS table of GAM LUP HD140008.fit FITS table of PSI-2 LUP HD140784.fit FITS table of HR5860 HD141637.fit FITS table of 1 SCO HD142114.fit FITS table of 2 SCO HD142165.fit FITS table of HR5906 HD142184.fit FITS table of HR5907 HD142250.fit FITS table of HR5910 HD142301.fit FITS table of 3 SCO HD142883.fit FITS table of HR5934 HD142983.fit FITS table of 48LIB HD142990.fit FITS table of HR5942 HD143018.fit FITS table of PISCO HD143118.fit FITS table of ETA LUP HD143699.fit FITS table of HR5967 HD144294.fit FITS table of THT LUP HD144661.fit FITS table of HR5998 HD145842.fit FITS table of THT NOR HD147152.fit FITS table of HR6083 HD147165.fit FITS table of SIG SCO HD147894.fit FITS table of HD147894 HD147971.fit FITS table of EPS NOR HD148478.fit FITS table of ALF SCO HD148605.fit FITS table of 22SCO HD149038.fit FITS table of MUNOR HD149404.fit FITS table of HR6164 HD149438.fit FITS table of TAU SCO HD149499.fit FITS table of HD149499 HD149711.fit FITS table of HR6174 HD149757.fit FITS table of ZET OPH HD150041.fit FITS table of HD150041 HD150136.fit FITS table of HR6187 HD150168.fit FITS table of HR6188 HD150898.fit FITS table of HR6219 HD151515.fit FITS table of HD151515 HD151804.fit FITS table of HR6245 HD151890.fit FITS table of MU-1 SCO HD151932.fit FITS table of HR6249 HD151985.fit FITS table of MU-2 SCO HD152236.fit FITS table of ZET-1 SCO HD152408.fit FITS table of HR6272 HD152478.fit FITS table of HR6274 HD153261.fit FITS table of HR6304 HD153716.fit FITS table of HR6320 HD153919.fit FITS table of HD153919 HD154090.fit FITS table of HR6334 HD155806.fit FITS table of HR6397 HD155889.fit FITS table of HD155889 HD156385.fit FITS table of HD156385 HD157042.fit FITS table of IOT ARA HD157056.fit FITS table of THT OPH HD157792.fit FITS table of 44OPH HD157832.fit FITS table of HD157832 HD157864.fit FITS table of HR6490 HD157978.fit FITS table of HR6497 HD158408.fit FITS table of UPS SCO HD158643.fit FITS table of 51OPH HD158704.fit FITS table of HR6520 HD158926.fit FITS table of LAM SCO HD159532.fit FITS table of THT SCO HD162978.fit FITS table of HR6672 HD163472.fit FITS table of HR6684 HD164402.fit FITS table of HR6716 HD164447.fit FITS table of HR6720 HD164577.fit FITS table of 68OPH HD164794.fit FITS table of 9 SGR HD164852.fit FITS table of 96HER HD165016.fit FITS table of HD165016 HD165024.fit FITS table of THT ARA HD165763.fit FITS table of HD165763 HD166182.fit FITS table of 102 HER HD166937.fit FITS table of MUSGR HD167263.fit FITS table of 16SGR HD167264.fit FITS table of 15SGR HD168905.fit FITS table of HR6875 HD169022.fit FITS table of EPS SGR HD169467.fit FITS table of ALF TEL HD170465.fit FITS table of DEL-1 TEL HD171034.fit FITS table of HR6960 HD172167.fit FITS table of ALF LYR HD173417.fit FITS table of HR7044 HD173648.fit FITS table of ZET LYR HD173948.fit FITS table of LAM PAV HD174179.fit FITS table of HR7081 HD174585.fit FITS table of 8 LYR HD174638.fit FITS table of BET LYR(.2 HD174638.fit FITS table of BET LYR(.5 HD174959.fit FITS table of HR7115 HD175426.fit FITS table of DEL-1 LYR HD175876.fit FITS table of HD175876 HD176318.fit FITS table of HR7174 HD176437.fit FITS table of GAM LYR HD177724.fit FITS table of ZET AQL HD181454.fit FITS table of BET-1 SGR HD181623.fit FITS table of BET-2 SGR HD181869.fit FITS table of ALF SGR HD183007.fit FITS table of HR7392 HD184905.fit FITS table of V1264 CYG HD185872.fit FITS table of 14CYG HD186618.fit FITS table of HD186618 HD187459.fit FITS table of HR7551 HD187879.fit FITS table of V380 CYG HD188209.fit FITS table of HR7589 HD188252.fit FITS table of HR7591 HD188439.fit FITS table of V819 CYG HD188892.fit FITS table of 22CYG HD189687.fit FITS table of 25CYG HD191610.fit FITS table of 28CYG HD192103.fit FITS table of V1042 CYG HD192163.fit FITS table of HD192163 HD192577.fit FITS table of 31CYG HD192909.fit FITS table of 32CYG HD193182.fit FITS table of HD193182 HD193237.fit FITS table of P CYG HD193369.fit FITS table of 36CYG HD193536.fit FITS table of HR7777 HD194335.fit FITS table of HR7807 HD197345.fit FITS table of ALF CYG HD199081.fit FITS table of 57CYG HD199579.fit FITS table of HR8023 HD200310.fit FITS table of 60CYG HD200595.fit FITS table of HR8064 HD201733.fit FITS table of HR8103 HD201819.fit FITS table of HR8105 HD202214.fit FITS table of HR8119 HD202347.fit FITS table of HD202347 HD202904.fit FITS table of UPS CYG HD203064.fit FITS table of 68CYG HD203280.fit FITS table of ALF CEP HD203338.fit FITS table of HR8164 HD203467.fit FITS table of 6 CEP HD204172.fit FITS table of 69CYG HD204403.fit FITS table of 70CYG HD205021.fit FITS table of BET CEP HD205139.fit FITS table of HR8243 HD205314.fit FITS table of HR8246 HD206165.fit FITS table of 9 CEP HD206267.fit FITS table of HR8281 HD206365.fit FITS table of HD206365 HD206672.fit FITS table of PI-1 CYG HD206696.fit FITS table of HD206696 HD207330.fit FITS table of PI-2 CYG HD208682.fit FITS table of HR8375 HD208816.fit FITS table of VVCEP HD208947.fit FITS table of HR8384 HD209339.fit FITS table of HR8399 HD209481.fit FITS table of 14CEP HD209790.fit FITS table of XICEP HD209975.fit FITS table of 19CEP HD210839.fit FITS table of LAM CEP HD211242.fit FITS table of HR8490 HD212120.fit FITS table of 2 LAC HD212593.fit FITS table of 4 LAC HD212883.fit FITS table of HR8549 HD212978.fit FITS table of HR8553 HD213310.fit FITS table of 5 LAC HD214168.fit FITS table of 8LAC HD214263.fit FITS table of HD214263 HD214680.fit FITS table of 10LAC HD214993.fit FITS table of 12DD LAC HD216916.fit FITS table of 16EN LAC HD217050.fit FITS table of EWLAC HD217675.fit FITS table of OMI AND HD217943.fit FITS table of HR8777 HD218045.fit FITS table of ALF PEG HD218376.fit FITS table of 1CAS HD218440.fit FITS table of HR8803 HD218537.fit FITS table of HR8808 HD219634.fit FITS table of HR8854 HD220057.fit FITS table of HD220057 HD221253.fit FITS table of ARCAS HD222109.fit FITS table of HR8962 HD222173.fit FITS table of IOT AND HD222439.fit FITS table of KAP AND HD224572.fit FITS table of SIG CAS Paul Kuin and C.-H. Joseph Lyu Hughes STX/NASA ADC 1997 Jan 29 The original ADC documentation by Robert S.H. and L.E. Brotzman (1984) and the catalog by Henize et al. (1979) were used to create this ReadMe file. UNKNOWN UNKNOWN The S-019 catalogue was received from S. Parsons by the Astronomical Data Center (ADC), NASA Goddard Flight Center, on several tapes in 1979. The treatment of the exposure data file was straightforward, and will not be discussed here. The spectrophotometric data was received in five files formatted for direct dumping to a printer to produce the catalogue as originally printed. The format has been radically changed. The data for each star have been put into a single record. In order to shorten the records to the degree possible, the flux data format has been condensed, mostly through the implicit representation of wavelength by the location of each datum in the record. No data have been changed or edited in regard to their content. The format was designed in order to simplify the structure of any Fortran program that would use the data by making it possible for one Fortran READ statement to store in variables all of the required data for any given star. Prints of the S-019 fields can be obtained from the National Space Science Data Center, NASA Goddard Space Flight Center, Greenbelt, MD 20771. This section describes the flux adjustment factor given in the first file (see data.dat, bytes 206-213). This explanation is partly quoted and partly paraphrased from the published catalogue. "The [flux adjustment] factor is determined by comparison at selected wavelengths between S-019 fluxes resulting from the adopted calibration and one of the following cases: (a) The flux measured by the S2/68 spectrometer on the TD-1 satellite (Jamar et al. 1976; Willis and Wilson 1978). (b) The flux measured by the WEP spectrometer on OAO-2 (Code and Meade 1976), but adjusted by as much as 25 percent to agree with TD-1 fluxes on the average. (c) The flux computed from (i) intrinsic UV colors derived from TD-1 fluxes as a function of spectral type (Nandy et al. 1976), from (ii) the visual magnitude, and from (iii) interstellar extinction corrections using E(B-V) defined by the Q method from UBV photometry (Johnson 1958). (d) The flux from model atmospheres (Kurucz et al. 1974) and from visual magnitude." Table 1. Flux Adjustment Factor Notation. r is the flux adjustment factor given in bytes 207-210 of the data fille (data.dat) The associated notations, described in this table, are given in bytes 206 and 211-213. Previous cases (a) - (d) are adopted here. NOTATION DESCRIPTION r: Adjustment factor determined for case (c). This method is restricted to spectral classes earlier than A0. (r) Adjustment factor determined for case (d). Used for stars in spectral classes A0 - A7 not measured by TD-1 or OAO-2. r+- Denotes a significant slope in the residual leading to a range on the order of 0.2 to 0.3 dex from the shortest to the longest wavelengths. A weighted mean r value is given. <r> The r value is predicted from appropriate shifts dependent on frame number and plate position for stars for which the r value could not be determined directly. See Henize et al. (1979), pp. 30-31, for more details. r:: Adjustment factor determined for cases (c) and (d) when there is uncertainty about the appropriate intrinsic colors. The estimated color and predicted log r were averaged to obtain the final r value presented in the catalogue. Table 2. Dummy Data Points. This table refers to bytes 214 - 5213, offsets +1 to +4, in data.dat. RECORD NO. STAR LAMBDA (A) ergs cm-2 s-1 A-1 147 HD 55879 1384 1.23 x 10-24 1398 1.23 x 10-24 1402 1.23 x 10-24 1404 1.23 x 10-24 171 HD 58978 1394 9.89 x 10-25 1404 9.89 x 10-25 207 HD 69106 1550 1.50 x 10-24 1552 1.50 x 10-24 Table 3. The stars in this catalog HDnumber Alt.name HDnumber Alt.name HDnumber Alt.name HDnumber Alt.name HD 358 ALF AND HD 432 BET CAS HD 593 HD593 HD 1337 AO CAS HD 1976 HR 91 HD 2054 HR 96 HD 2772 LAM CAS HD 2905 KAP CAS HD 3240 HR 144 HD 3360 ZET CAS HD 4142 HR 189 HD 4180 OMI CAS HD 5394 GAM CAS HD 5408 HR 266 HD 10144 ALF ERI HD 10516 PHI PER HD 16349 HD16349 HD 18925 GAM PER HD 19268 HR 930 HD 19356 BET PER HD 20191 HD20191 HD 20283 HR 979 HD 20677 32 PER HD 20809 HR 1011 HD 20902 ALF PER HD 21364 XI TAU HD 21428 34 PER HD 21551 HR 1051 HD 21686 4 TAU HD 21699 HR 1063 HD 21856 HR 1074 HD 21933 6 TAU HD 22192 PSI PER HD 22780 HR 1113 HD 22928 DEL PER HD 22951 40 PER HD 23193 HR 1133 HD 23302 17 TAU HD 23630 ETA TAU HD 23753 HR 1172 HD 23848 42 PER HD 23985 HR 1188 HD 24398 ZET PER HD 24504 HR 1207 HD 24534 X PER HD 24640 HR 1215 HD 24912 XI PER HD 25940 48 PER HD 27045 OMG TAU HD 27295 53 TAU HD 27309 56 TAU HD 27396 53 PER HD 27934 KAP TAU HD 27946 67 TAU HD 28024 UPS TAU HD 28319 THT-2 TAU HD 28546 81 TAU HD 28556 83 TAU HD 28879 HD28879 HD 28910 RHO TAU HD 29479 SIG-1 TAU HD 29488 SIG-2 TAU HD 31512 62 ERI HD 32068 ZET AUR HD 32249 PSI ERI HD 32630 ETA AUR HD 32964 66 ERI HD 33111 BET ERI HD 33328 LAM ERI HD 33904 MU LEP HD 33948 HR 1704 HD 34029 ALF AUR HD 34085 BET ORI HD 34503 TAU ORI HD 34816 LAM LEP HD 35007 HR 1764 HD 35039 22 ORI HD 35149 23 ORI HD 35299 HR 1781 HD 35337 8 LEP HD 35439 25 ORI HD 35468 GAM ORI HD 35575 HD35575 HD 35588 HR 1803 HD 35708 114 TAU HD 35715 PSI ORI HD 35912 HR 1820 HD 36267 32 ORI HD 36285 HR 1840 HD 36351 33 ORI HD 36430 HR 1848 HD 36486 DEL ORI HD 36486 DEL ORI HD 36512 UPS ORI HD 36591 HR 1861 HD 36695 VV ORI HD 36779 HR 1873 HD 36822 PHI-1 ORI HD 36827 HD36827 HD 36861 LAM ORI HD 36895 HD36895 HD 36960 HR 1887+86HD 37041 THT-2 ORI HD 37043 IOT ORI HD 37128 EPS ORI HD 37150 HR 1906 HD 37202 ZET TAU HD 37209 HR 1911 HD 37269 26 AUR HD 37303 HR 1918 HD 37468 SIG ORI HD 37481 HR 1933 HD 37490 OMG ORI HD 37507 49 ORI HD 37742 ZET ORI HD 37744 HR 1950 HD 37756 HR 1952 HD 39985 HR 2075 HD 42087 3 GEM HD 42216 HD42216 HD 42933 DEL PIC HD 45057 HD45057 HD 45348 ALF CAR HD 45789 HD45789 HD 45995 HR 2370 HD 46300 13 MON HD 46885 HR 2413 HD 46966 HD46966 HD 47129 HR 2422 HD 47417 HD47417 HD 47839 15 S MON HD 48099 HR 2467 HD 48917 10 CMA HD 49961 HD49961 HD 50013 KAP CMA HD 50123 HR 2545 HD 51411 HR 2598 HD 52140 HR 2621 HD 52670 HR 2640 HD 53138 OMI-2 CMA HD 53344 HD53344 HD 54605 DEL CMA HD 54893 HR 2702 HD 54912 HR 2704 HD 55522 26 CMA HD 55857 HR 2734 HD 55879 HR 2739 HD 55958 HR 2741 HD 55985 HR 2743 HD 56014 27 CMA HD 56094 HD56094 HD 56139 OMG CMA HD 56342 HR 2756 HD 56455 HR 2761 HD 56554 HD56554 HD 56779 HR 2770 HD 56876 HR 2774 HD 57060 29 UW CMA HD 57061 TAU CMA HD 57150 HR 2787 HD 57193 HD57193 HD 57219 HR 2790 HD 57593 HR 2800 HD 58011 HD58011 HD 58260 HD58260 HD 58286 HR 2823 HD 58325 HR 2824 HD 58350 ETA CMA HD 58420 HR 2829 HD 58612 HR 2841 HD 58978 HR 2855 HD 59026 HR 2856 HD 59136 HR 2860 HD 59499 HR 2870+71HD 59527 HD59527 HD 59550 HR 2873 HD 59864 HD59864 HD 60098 HR 2885 HD 60168 HR 2889 HD 60312 HR 2895 HD 60344 HD60344 HD 60606 HR 2911 HD 61071 HD61071 HD 61330 HR 2937 HD 61429 HR 2944 HD 62315 HD62315 HD 62623 3 PUP HD 62747 HR 3004 HD 63308 HR 3025 HD 63425 HD63425 HD 63462 OMI PUP HD 63465 HR 3035 HD 63868 HD63868 HD 64365 HR 3078 HD 64440 HR 3080 HD 65315 HR 3107 HD 66624 HR 3162 HD 66811 ZET PUP HD 68092 HD68092 HD 68161 HR 3203 HD 68273 GAM VEL HD 68324 HR 3213 HD 68657 HR 3227 HD 68761 HD68761 HD 68895 HR 3234 HD 68980 HR 3237 HD 69106 HD69106 HD 69144 HR 3244 HD 69168 HD69168 HD 69302 HR 3250 HD 69404 HD69404 HD 69973 HD69973 HD 70309 HD70309 HD 70556 HR 3283 HD 70930 HR 3294 HD 71935 HR 3350 HD 72108 HR 3358 HD 72232 HR 3363 HD 72737 HR 3386 HD 73105 HD73105 HD 74071 HR 3440 HD 74146 HR 3442 HD 74195 OMI VEL HD 74319 HD74319 HD 74371 HR 3456 HD 74956 DEL VEL HD 75241 HD75241 HD 75821 HR 3527 HD 76004 HD76004 HD 76538 HR 3560 HD 76566 HR 3562 HD 76728 HR 3571 HD 77002 HR 3582 HD 77320 HR 3593 HD 77475 HR 3600 HD 78616 HD78616 HD 79186 HR 3654 HD 79351 A. CAR HD 79416 HR 3661 HD 79447 HR 3663 HD 79694 HR 3672 HD 79735 HR 3674 HD 80404 IOT CAR HD 83944 HR 3856 HD 83979 ZET CHA HD 84228 HR 3868 HD 84809 HR 3883 HD 85871 HR 3920 HD 86440 PHI VEL HD 87737 ETA LEO HD 87901 ALF LEO HD 90853 HR 4114 HD 91316 RHO LEO HD 91465 PP CAR HD 92664 HR 4185 HD 92740 HR 4188 HD 93030 THT CAR HD 93194 HR 4205 HD 93845 DEL-2 CHA HD 97583 HR 4355 HD100841 LAM CEN HD101379 HR 4492 HD102249 LAM MUS HD102647 BET LEO HD103079 HR 4549 HD106983 ZET CRU HD108248 ALF CRU HD110335 HR 4823 HD112078 LAM CRU HD113904 THT MUS HD114529 HR 4975 HD114911 ETA MUS HD115846 HD115846 HD116658 ALF VIR HD117651 HR 5093 HD120640 HR 5206 HD120991 HR 5223 HD121483 HD121483 HD121790 UPS-1 CEN HD122451 BET CEN HD124367 HR 5316 HD125238 IOT LUP HD125288 HR 5358 HD125721 HR 5375 HD125823 HR 5378 HD126341 TAU-1 LUP HD126759 HD126759 HD126983 HR 5413 HD127381 SIG LUP HD127971 HR 5439 HD127972 ETA CEN HD128345 RHO LUP HD128620 ALF CEN HD128974 HR 5466 HD129056 ALF LUP HD129092 HD129092 HD129116 HR 5471 HD129422 HR 5482 HD129929 HD129929 HD130559 MU LIB HD130701 AX CIR HD130807 OMI LUP HD130819 ALF-1 LIB HD130841 ALF-2 LIB HD131120 HR 5543 HD131492 THT CIR HD132058 BET LUP HD132200 KAP CEN HD133738 HD133738 HD133955 LAM LUP HD134657 HD134657 HD134687 HR 5651 HD135160 HR 5661 HD135240 DEL CIR HD135591 HR 5680 HD135734 MU LUP HD135917 HD135917 HD136415 GAM CIR HD136504 EPS LUP HD138690 GAM LUP HD140008 PSI-2 LUP HD140784 HR 5860 HD141637 1 SCO HD142114 2 SCO HD142165 HR 5906 HD142184 HR 5907 HD142250 HR 5910 HD142301 3 SCO HD142883 HR 5934 HD142983 48 LIB HD142990 HR 5942 HD143018 PI SCO HD143118 ETA LUP HD143699 HR 5967 HD144294 THT LUP HD144661 HR 5998 HD145842 THT NOR HD147152 HR 6083 HD147165 SIG SCO HD147894 HD147894 HD147971 EPS NOR HD148478 ALF SCO HD148605 22 SCO HD149038 MU NOR HD149404 HR 6164 HD149438 TAU SCO HD149499 HD149499 HD149711 HR 6174 HD149757 ZET OPH HD150041 HD150041 HD150136 HR 6187 HD150168 HR 6188 HD150898 HR 6219 HD151515 HD151515 HD151804 HR 6245 HD151890 MU-1 SCO HD151932 HR 6249 HD151985 MU-2 SCO HD152236 ZET-1 SCO HD152408 HR 6272 HD152478 HR 6274 HD153261 HR 6304 HD153716 HR 6320 HD153919 HD153919 HD154090 HR 6334 HD155806 HR 6397 HD155889 HD155889 HD156385 HD156385 HD157042 IOT ARA HD157056 THT OPH HD157792 44 OPH HD157832 HD157832 HD157864 HR 6490 HD157978 HR 6497 HD158408 UPS SCO HD158643 51 OPH HD158704 HR 6520 HD158926 LAM SCO HD159532 THT SCO HD162978 HR 6672 HD163472 HR 6684 HD164402 HR 6716 HD164447 HR 6720 HD164577 68 OPH HD164794 9 SGR HD164852 96 HER HD165016 HD165016 HD165024 THT ARA HD165763 HD165763 HD166182 102 HER HD166937 MU SGR HD167263 16 SGR HD167264 15 SGR HD168905 HR 6875 HD169022 EPS SGR HD169467 ALF TEL HD170465 DEL-1 TEL HD171034 HR 6960 HD172167 ALF LYR HD173417 HR 7044 HD173648 ZET LYR HD173948 LAM PAV HD174179 HR 7081 HD174585 8 LYR HD174638 BET LYR(.2HD174638 BET LYR(.5HD174959 HR 7115 HD175426 DEL-1 LYR HD175876 HD175876 HD176318 HR 7174 HD176437 GAM LYR HD177724 ZET AQL HD181454 BET-1 SGR HD181623 BET-2 SGR HD181869 ALF SGR HD183007 HR 7392 HD184905 V1264 CYG HD185872 14 CYG HD186618 HD186618 HD187459 HR 7551 HD187879 V380 CYG HD188209 HR 7589 HD188252 HR 7591 HD188439 V819 CYG HD188892 22 CYG HD189687 25 CYG HD191610 28 CYG HD192103 V1042 CYG HD192163 HD192163 HD192577 31 CYG HD192909 32 CYG HD193182 HD193182 HD193237 P CYG HD193369 36 CYG HD193536 HR 7777 HD194335 HR 7807 HD197345 ALF CYG HD199081 57 CYG HD199579 HR 8023 HD200310 60 CYG HD200595 HR 8064 HD201733 HR 8103 HD201819 HR 8105 HD202214 HR 8119 HD202347 HD202347 HD202904 UPS CYG HD203064 68 CYG HD203280 ALF CEP HD203338 HR 8164 HD203467 6 CEP HD204172 69 CYG HD204403 70 CYG HD205021 BET CEP HD205139 HR 8243 HD205314 HR 8246 HD206165 9 CEP HD206267 HR 8281 HD206365 HD206365 HD206672 PI-1 CYG HD206696 HD206696 HD207330 PI-2 CYG HD208682 HR 8375 HD208816 VV CEP HD208947 HR 8384 HD209339 HR 8399 HD209481 14 CEP HD209790 XI CEP HD209975 19 CEP HD210839 LAM CEP HD211242 HR 8490 HD212120 2 LAC HD212593 4 LAC HD212883 HR 8549 HD212978 HR 8553 HD213310 5 LAC HD214168 8 LAC HD214263 HD214263 HD214680 10 LAC HD214993 12 DD LAC HD216916 16 EN LAC HD217050 EW LAC HD217675 OMI AND HD217943 HR 8777 HD218045 ALF PEG HD218376 1 CAS HD218440 HR 8803 HD218537 HR 8808 HD219634 HR 8854 HD220057 HD220057 HD221253 AR CAS HD222109 HR 8962 HD222173 IOT AND HD222439 KAP AND HD224572 SIG CAS III_86.xml Stellar Spectrophotometric Atlas 3088 III/88 Stellar Spectrophotometric Atlas Stellar Spectrophotometric Atlas J E Gunn L L Stryker Astrophys. J. Suppl. Ser. 52 121 1983 1983ApJS...52..121G Spectrophotometry The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.
Details about each star No Running number --- ID Star name --- Sp Spectral type --- AVref Absorption from reference mag AP Aperture size arcsec G Code for green filter --- R Code for red filter --- B Code for blue filter --- obj Object code --- day_co Code for day of observation --- V Magnitude from scan number=1 The magnitudes and colors are derived from the scans. Although they are given to 0.001 mag. they are accurate to only 0.1 mag. mag AV Visual absorption number=1 The magnitudes and colors are derived from the scans. Although they are given to 0.001 mag. they are accurate to only 0.1 mag. mag U-B U-B color from scan number=2 The colors were derived from the scans convolved with the standard filter functions mag B-V B-V color from scan number=2 The colors were derived from the scans convolved with the standard filter functions mag V-R V-R color from scan number=2 The colors were derived from the scans convolved with the standard filter functions mag R-I R-I color from scan number=2 The colors were derived from the scans convolved with the standard filter functions mag amass Airmass number=3 Secant of the zenith distance at mid-observation --- plot Internal data used for plotting --- RArad Right ascension (1950) rad DErad Declination (1950) rad cosb Cosecant of galactic latitude --- Miscellaneous data for each star No Running number --- tape Internal tape number --- atm 777 if atmospheric cycles have been removed; otherwise, 0 number=1 See Gunn and Stryker 1983 --- red 888 if problems with red. number=1 See Gunn and Stryker 1983 --- c33-37 Continuum color: 33-37 mag c37-40 Continuum color: 37-40 mag c40-46 Continuum color: 40-46 mag c46-V Continuum color: 46-V mag cV-70 Continuum color: V-70 mag c70-87 Continuum color: 70-80 mag c87-99 Continuum color: 87-99 mag Bal_brk Balmer break index mag inCN38+ CN38 index mag in41-42 41-42 index mag inCaH CaH index mag inCaK CaK index mag inTi61+ Ti61+ index mag inTi71+ Ti71+ index mag inCa42 Ca42 index mag inCH43 CH43 index mag inMg51 Mg51 index mag inNaD NaD index mag Fluxes Mean error for each flux No Running number --- lambda Wavelength for first flux value number=1 In each record, the wavelength of the ith record = lambda+10(i-1) for lambda less than 5745 = lambda+20(i-1) for lambda greater than 5745 Note for the 25th record for each star (starting with the flux for 5660), the interval changes within the record. Specifically, the 10th flux is for 5760. 0.1nm flux1 Flux for the 1st wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux2 Flux for the 2nd wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux3 Flux for the 3rd wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux4 Flux for the 4th wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux5 Flux for the 5th wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux6 Flux for the 6th wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux7 Flux for the 7th wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux8 Flux for the 8th wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux9 Flux for the 9th wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz flux10 Flux for the 10th wavelength number=2 The fluxes are apparently divided by 3.67 to normalize them to a mag=0 star. 10-20mW/m2/Hz N. G. Roman SSDOO/ADC 1999 Mar 10 by W.H. Warren: Appreciation is expressed to Dr. Linda L. Stryker for supplying the original magnetic tape of the atlas, for sending a preprint of the published paper, and for replying quickly in response to questions about the format description. Dr. Stryker kindly reviewed the completed document. UNKNOWN UNKNOWN As noted below, the ADC archived and documented this catalog in 1984. The CDS built the "catalog" file by incorporating the error mentioned as a "Note added in proof" concerning the HD number of star number 115, and by concatenating the 142 consecutive records making up one spectrum. The undersigned broke these again into four arrays, each with a number of records for each star. UNKNOWN UNKNOWN Excerpt from the original ADC document, prepared by Wayne H. Warren Jr: The tape version of the Stellar Spectrophotometric Atlas was received from Dr. L. L. Stryker of the Dominion Astrophysical Observatory on 21 October 1982. A brief description of the format was supplied with the tape, the latter being written with 84-byte logical records having the digits "0084" in bytes 1-4 of each record. The atlas was transferred to disk storage and changed to 80-byte logical records by elimination of the "0084". A computer program to print and plot spectra from the atlas is available and can be obtained from Dr. Stryker. An error in the name identification for star number 115 has been found and transmitted by Dr. Stryker: HD 113439 should be HD 113493. The error was not corrected in the first adc version; it was corrected by the CDS.. The following message was recieved from Dawn Lenz on Mar-22-1995: This is in response to your request (9 feb) for any addtional information I could find about the Gunn-Stryker catalog (A3088). Jim Gunn tells me that "the fluxes are fluxes per unit frequency F_nu, corrected for the atmosphere AND for galactic extinction. They are normalized so that the V magnitude of a star with those fluxes is zero." III_88.xml A Catalog of Stellar Spectrophotometric Data 3089 III/89 Stellar Spectrophotometry A Catalog of Stellar Spectrophotometric Data S J Adelman D M Pyper S N Shore R E White W H Warren Astron. Astrophys. Suppl. Ser. 81 221 1989 1989A&AS...81..221A Spectrophotometry The catalog is a collection of spectrophotometric measurements obtained with rotating grating scanners attached to various telescopes at the Kitt Peak National, Mount Wilson, and Palomar Observatories. The observations were made during the 1970s and early 1980s, both individually and jointly, by S.J. Adelman, D.M. Pyper, S.N. Shore, and R.E. White. All measurements were calibrated with the fluxes of Alpha Lyrae (Vega) as presented by Hayes and Latham (1975ApJ...197..593H). There are 1134 observations concerning 207 individual stars.
List of all observations RAh Right Ascension 2000 (hours) number=1 Positions from SIMBAD, added at CDS. h RAm Right Ascension 2000 (minutes) number=1 Positions from SIMBAD, added at CDS. min RAs Right Ascension 2000 (seconds) number=1 Positions from SIMBAD, added at CDS. s DE- Declination 2000 (sign) number=1 Positions from SIMBAD, added at CDS. --- DEd Declination 2000 (degrees) number=1 Positions from SIMBAD, added at CDS. deg DEm Declination 2000 (minutes) number=1 Positions from SIMBAD, added at CDS. arcmin DEs Declination 2000 (seconds) number=1 Positions from SIMBAD, added at CDS. arcsec Name Star name --- HD/BD HD or BD Designation --- HR HR (Bright Star) Designation --- m_HR Component designation --- B-V Colour index mag SpType Spectral Type and comments --- BW Bandwidth (in the second order) 0.1nm Paper Paper number detailed in file refs.dat (unknown only for star Lam Cnc #391) --- NS Number of separate scans included in the average spectrum --- HJD Heliocentric Julian Date of Observation (for variables) d NWL Number of data points in data.dat number=2 Each data point consists in a pair of wavelength value (in Angstroems) and normalized magnitude (normalized to m(5000A) = 0) --- m5000 Magnitude at 500nm mag List of papers referenced Paper Paper number, repated for several lines --- Text Text of reference, starting by the bibcode when the paper was effectively published --- text.txt Original Description of catalog.dat adc.doc Original ADC Documentation of data.dat and text.txt adc.tex LaTeX version of adc.doc Francois Ochsenbein CDS 1998 May 06 UNKNOWN UNKNOWN * January 1990, Wayne H. Warren (from "adc.doc" file): The text and data files were prepared initially at The Citadel by S. J. Adelman following discussions about an acceptable structure and format for the catalog. Proofreading was done with the assistance of Carol J. Adelman and Jeffrey A. Garret. The data were transferred to the Astronomical Data Center via BITnet. Extensive checks of the header records resulted in minor corrections and changes, e.g., to correct shifted data and to insert mixed case characters where appropriate. * May 1998, F. Ochsenbein: the files "stars.dat" and "refs.dat" have been created from the "data.dat" headers and the "text.txt" file. The positions were extracted from the SIMBAD data-base. III_89.xml A Library of Stellar Spectra 3092 III/92 A Library of Stellar Spectra A Library of Stellar Spectra G H Jacoby D A Hunter C A Christian Astrophys. J. Suppl. Ser. 56 257 1984 1984ApJS...56..257J III/83 : IUE Low-Dispersion Reference Atlas I, Normal Stars (Heck+ 1984) III/88 : Stellar Spectrophotometric Atlas (Gunn+ 1983) III/124 : Spectrophotometry of 60 stars (Kiehling, 1987) III/166 : A New Library of Optical Spectra (Silva+ 1992) III/196 : Near-IR stellar spectra from 1.428 to 2.5 um (Lancon+ 1996) VI/50 : Intensity Distribution of Normal Stars (Sviderskiene, 1988) J/PASP/110/863 : A Stellar Spectral Flux Library 1150-25000{AA} (Pickles 1998) Jacoby G.H., Hunter D.A. and Christian C.A. 1984, A Library of Stellar Spectra, Astrophys. J. Suppl. Ser. 56, 278. (1984ApJS...56..257J) Spectrophotometry The machine-readable version of the library contains digital spectra of 161 stars of spectral types O through M and luminosity classes I, III, and V. Most stars are of solar metallicity, although two were chosen specifically for low metallicity. The data were obtained with the Intensified Reticon Scanner on the #1 91-cm telescope at Kitt Peak National Observatory. The scans cover the wavelength range 3510-7427 angstroms, with a resolution of approximately 4.5 angstroms, while the typical photometric uncertainty of each resolution element is about 1 percent and broadband variations are < 3 percent.
Information on each star Name Star identification (HD, BD, SAO, misc.) Positions with variable precision derived from SIMBAD. The following four stars could not be identified, and have the RA and Dec columns blank: TR A 14 (G4 V star) HD 249240 (G7 III star), the HD classifies this star as A2. The star could be HD 24924 (K0 star, Vmag=9.39, at 03 57 35.5 -01 58 30 (2000)). LSIV P 24 (B9 I) 42 LSI (A2 I) --- Sp Adopted spectral type. --- Lum Adopted luminosity class --- Sp1 Spectral type from lit. if different --- Lum1 Luminosity class from lit. if different --- E(B-V) Derived color excess E(B-V) Derived color excess, E(B-V), used to to deredden the spectrum. mag (U-B)s U-B color synthesized from the spectrum. mag (B-V)s B-V color synthesized from the spectrum. mag (U-B)0 Dereddened color derived from (U-B)s mag (B-V)0 Dereddened color derived from (B-V)s --- U-B U-B color taken from the literature. mag B-V B-V color taken from the literature. mag lambda1 Wavelength of first pixel 0.1nm Dlambda Wavelength increment per pixel 0.1nm RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec The Library of Stellar Spectra, flux data ID Star identification from headers.dat --- F(i) Flux values F(i) in erg/cm2/s/Angstrom Flux values F(i) in erg/cm2/s/Angstrom at wavelengths: lambda(i) = lambda1 + (i-1+[7*(L-1)])*Dlambda where L is the number of the line for the star of interest. There are 400 lines of fluxes for each star. Hence, L is the line number in the file, modulo 400. In the final record for each star, the seventh flux on the record appears blank. 10mW/m2/nm Julie Anne Watko SSDOO/ADC Francois Ochsenbein CDS 1998 Oct 06 Documentation for the original version was written by Wayne H. Warren, Jr. [NSSDC/WDC-A-R&S] November 1984. This ReadMe file is a revision of Dr. Warren's original document and an Intro document [CDS] 24-May-1993 to the current CDS standard. UNKNOWN UNKNOWN * 24-May-1993 [CDS] The original data pertaining to each star were contained in a group of 352 data records. The first two (header) records contained general information about the star, such as identification, spectral type, UBV colors and reddening, intrinsic UBV colors, and wavelength information. Records 3-352 contained 2799 flux values in groups of eight fluxes per record. The original file can easily be rebuilt by splitting each record in 352 80-bytes records; this split is straightforward on Unix workstations with the "fold" command. * 23-Aug-1996 Julie Anne Watko [SSDOO/ADC] The previous version of this catalog contained all data for each star on a single record. To provide a more useful lrecl, the long records were folded into 70-byte records using the Unix fold command. J.A. Watko [ADC] used IDL to insert star identification into the first 10 bytes of each record and to create a separate file of header data. * 06-Oct-1998 [CDS] Positions of the stars were added when possible --- four stars could not be recognized. III_92.xml Bibliography of Individual Radial Velocities for Stars in Open Clusters II. NGC and IC Clusters 3097A III/97A Radial Velocities in open clusters Bibliography of Individual Radial Velocities for Stars in Open Clusters II. NGC and IC Clusters J -C Mermilliod Bull. Inform. CDS 26 9 1984 1984BICDS..26....9M Bibliography Clusters, open Radial velocities This second part of the bibliography contains 6504 individual radial velocities for 774 stars in 78 open clusters. It is devoted to NGC and IC open clusters. The first part (Mermilliod J.-C., 1979, Bull. Inform. CDS 16,2; catalogue III/55/) contains the data for five nearby open clusters. The collected data have been found in the literature published from 1900 to the end of 1983. This catalog contains also unpublished data which have been delivered to Mermilliod by several authors.
The catalogue data LID Designation in Geneva/Lausanne system Designation in Geneva/Lausanne system 2.XXXXBBBB = NGC cluster number XXXX, 3.XXXXBBBB = IC cluster number XXXX (see file "refs.dat" for numbering BBBB) --- m_LID Component of star --- JD Julian date of the observation d RV Radial velocity km/s e_RV Probable error on RV km/s Lines Number of lines observed --- Disp Dispersion in A/mm 0.1nm/mm n_RV Technique used Technique used: OP = objective prism PE = photoelectric scanner RE = Reticon velocity --- Ref Reference --- References of star designations in clusters Ident +2.=NGC Cluster; +3.=IC Cluster --- Num Cluster number --- Suffix Suffix --- rem Remarks --- C.-H. Joseph Lyu Hughes STX/NASA Francois Ochsenbein CDS 1997 Jan 07 The original Intro document by J. C. Mermilliod (1984) was used to create this ReadMe file. J.-C. Mermilliod Institut d'Astronomie de l'Universite de Lausanne CH - 1290 CHAVANNES - DES - BOIS UNKNOWN UNKNOWN The decimal point has been added in "Disp" column, and blanks between signs and numbers in column "RV" were removed. III_97A.xml Radial Velocities of Southern Stars Obtained with the Photoelectric Scanner CORAVEL. III. 790 Late-Type Bright Stars 3105 III/105 Radial Velocities of Southern Stars with CORAVEL Radial Velocities of Southern Stars Obtained with the Photoelectric Scanner CORAVEL. III. 790 Late-Type Bright Stars J Andersen B Nordstroem A Ardeberg W Benz M Imbert H Lindgre N Martin E Maurice M Mayor L Prevot Astron. & Astrophys. Suppl. 59 15 1985 1985A&AS...59...15A Stars, bright Radial velocities The catalog contains 1595 photoelectric radial-velocity observations for 790 bright southern stars of spectral type F5 and later. One of the purposes of this project is to make a complete southern sky radial velocity coverage using the second CORAVEL photoelectric radial-velocity scanner. The first CORAVEL operating at Observatoire de Haute Provence was used to observe the stars in the Northern Hemisphere. Two CORAVEL observations per star were made with CORAVEL photoelectric radial- velocity scanner on the Danish 1.54-m telescope at ESO, La Silla, Chile. The mean velocities are accurate to about 0.15 km/sec r.m.s. for sharp-lined constant stars, errors increasing somewhat for stars with significant rotation. The present data complete and supersede the preliminary data for 500 stars supplied in advance of publications for inclusions in the fourth edition of The Bright Star Catalogue. At the time this project was planned, there were still some 1500 stars in The Bright Star Catalogue for which no radial-velocity information was available -- virtually all of them in the Southern Hemisphere. For the stars of type F5 and later, photoelectric scanning techniques can be used with much increased efficiency and accuracy. The catalog includes HD numbers with component designation for visual binary components from Jeffers et al. (1963), HR numbers, FK4 or FK4 Supplement numbers, visual magnitudes, MK spectral classes, mean velocities, velocity variability parameters, rotation classes as assigned from the measured linewidths, and remarks and information for individual measurements in a separate file.
Mean Velocities HD HD number --- HDsuffix HD suffix Component designation from Jeffers et al. (1963) . --- HR HR number --- Vmag Visual magnitude From an updated version of the Bright Star Catalogue on magnetic tape supplied to the catalog authors by the Centre de Donnees Stellaires in 1981. mag Vflag Visual mag. flag "V" if the star is variable. --- Sp MK spectral class MK spectral class also from the magnetic tape version of the Bright Star Catalogue supplied by the CDS. --- RV Mean radial velocity km/s e_RV RV mean error Root mean square error in the mean radial velocity in km/s. Andersen and Nordstrom (1983a) and Andersen et al. (1985) for a discussion of sources of error and the derivation of the error estimate. km/s RVvar Velocity variability parameter Velocity variability parameter, defined as "the ratio ... between the actual r.m.s. dispersion (SigmaE) of the observed velocities and that (SigmaT) expected for a constant-velocity star on the basis of the uncertainty of each measurement, taking all error sources into account. For n = 2 observations, we adopt RVvar > 2.0 and RVvar > 3.0 as the criteria for possible and certain variability, respectively." See Andersen et al. (1985) for a brief discussion of the relationship between this parameter and the r.m.s. error in the mean velocity. --- NObs Number of obs. Number of observations contributing to the radial velocity in bytes 41-46. --- rem Notes Notes regarding variability. "REM" indicates that a remark concerning this object can be found in remarks.dat. --- Observations HD HD number --- HDsuffix HD suffix Component designation from Jeffers et al. (1963). --- JD Julian Date Heliocentric Julian date (-2,440,000) of the observation. --- RV Observed Radial velocity km/s e_RV Computed r.m.s. error in the RV km/s rem Remarks Remarks concerning this observation. "PR" and "SEC" indicate the primary and secondary components, respectively, of a double-line binary system. "REM" indicates that there is a remark about this observation in the remarks file. --- Remarks HD HD number --- HDsuffix HD suffix Component designation from Jeffers et al. (1963). --- rem Remark Text of the remark. When bytes 1-8 are blank this field continues the remark from the previous record. "BE" refers to Beavers and Eitter (1981). "AN" refers to Andersen and Nordstrom (1983c). A number in parentheses is a number of observations. --- C.-H. Joseph Lyu, Paul Kuin Hughes STX/NASA ADC 1997 Jan 07 The original ADC documentation by A. C. Raugh (1988) was used to create this ReadMe file by J. Lyu. UNKNOWN UNKNOWN Radial Velocities of Southern Stars Obtained with the Photoelectric Scanner CORAVEL. III. 790 Late-Type Bright Stars (RVSS3) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in July 1985. The tape contained three files: the first listing the radial velocity results, the second listing the observations, and the third containing the remarks, all formatted in the same manner as the published catalog. Several records containing descriptive information were deleted from the beginning of each file and blank columns were removed by means of an editor. III_105.xml Visual Multiples. VII. MK Classifications 3106 III/106 Visual Multiples. VII. MK Classifications Visual Multiples. VII. MK Classifications H A Abt Astrophys. J. Suppl. 45 437 1981 1981ApJS...45..437A Stars, double and multiple MK spectral classification Spectral types Classifications are given for 865 components of visual multiples; they show no systematic differences from the MK system, and the random errors are one subclass in type and two-thirds of a luminosity class. Fields given include ADS, HD and HR identification, MK classifications, luminosity classes, alternative names, selected published spectral types and references.
Data ID ADS number --- comp Component --- HD HD number --- HD_sep Separator --- HD_comp Second component HD number --- HR HR number --- HR_sep Seeparator --- HR_comp HR number of second component --- Sp Spectral type --- ot_Sp Other sp. types and their references --- N.G. Roman & Julie Anne Watko SSDOO/ADC 1997 Jul 24 III_106.xml Catalogue of Spectral and Luminosity classes of 10396 stars in Kapteyn areas 2-43 3112 III/112 Spectral Classes in Kapteyn areas 2-43 Catalogue of Spectral and Luminosity classes of 10396 stars in Kapteyn areas 2-43 R A Bartaya Bull. Abastumani Astrophys. Observ. 51 ??? ??? 1979 1979AbaOB..51....1B Catalogue of Spectral and Luminosity classes of 10396 stars in Kapteyn areas 2-43 R A Bartaya Bull. Inform. CDS 24 93 1983 1983BICDS Selected areas Spectral types The present catalogue is compiled on the basis of the spectral data obtained with the 70-cm meniscus telescope of Abastumani Astrophysical Observatory using the 8{deg} objective prism (dispersion 166{AA}/mm near H{gamma}; in the short-wave region, the spectrum extends up to 3500{AA}). We have confined ourselves to relatively bright stars (11.5 photographic mag.), whose spectra were obtained by us on Kodak IIa-O plates. The spectra were broadened up to 0.4mm for an exposure of 20min. We succeeded to carry out a quite homogeneous mass two-dimensional MK classification, separating also peculiar stars. In order to detect also H{alpha} emission stars and M, S, C type stars in the surveyed Kapteyn areas (KA), panchromatic plates were also taken. The catalogue contains 173 stars with peculiarities in the spectrum, in particular Ap, Am, BaII and composite spectrum stars, as well as 30 Be, 800 M-type, and a few S, R, N and WR stars. The data for all KA's are uniform not only in the sense of classification accuracy (the whole classification is done by one person - the author of the present catalogue), but also in the sense of penetration: the areas were photographed both on Kodak IIa-O and ORWO 2P-3 plates with the same maximum exposure for each plate and they all cover areas of 4.5x4.5{deg}. The errors of our determinations are: +/-0.6 for spectral subtype and +/-0.5 for luminosity class. The stars in the KA's are arranged in the Catalogue by increasing right ascension. The stars are numbered according to zones of 1{deg} in declination. The printed catalogue is provided with suitable stellar charts for separate KA's reproduced from the Lick Catalogue. The reference system on the charts refers to 1950 epoch and it is plotted according to the Smithsonian Astrophysical Observatory (SAO) catalogue.
The catalogue of spectral classes ComFlag '*' if a comment exists in file notes.dat --- ID Star Designation Each star is designated by 3 numbers separated by a blank "K D N", where K = Kaptyen area number (between 2 and 43) D = Declination zone (degrees) N = Running number within the zone. --- BD Designation on BD catalog --- HD Designation in HD (Cat. <III/135>) --- RAh Right Ascension 1950 (hours) from SAO h RAm Right Ascension 1950 (minutes) from SAO min RAs Right Ascension 1950 (seconds) from SAO s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) from SAO deg DEm Declination 1950 (minutes) from SAO arcmin DEs Declination 1950 (seconds) from SAO arcsec Pmag Photographic magnitude mag u_Pmag Uncertainty flag --- n_Pmag Variability flag --- SpType Spectral classification the spectrum is formatted as follows: +0 (byte 63): luminosity prefix (d g c) if any; +1 (byte 64): spectral temperature class +2 (byte 65): spectral temperature subclass +3 (byte 66): peculiarity +4 (bytes 67-69): luminosity class +7 (byte 70): '-' if luminosity class is uncertain +8 (byte 71): '+' is spectrum is double +9 (byte 72): secondary spectrum, if existing --- u_SpType Uncertainty flag on SpType --- BSD Bergedorfer Spektral Durchmusterung The Bergedorfer Spektral Durchmusterung was prepared by Schwassmann A. and van Rhijn P.J., and published by the Hamburger Sternwarte in Bergedorf between 1935 and 1953 in 5 volumes. Note that only the second part of the BSD designation is stored in this column: the Kapteyn Area number (the first number in the ID column) must be added in front of the contents of this column to generate the complete BSD designation. --- SAO SAO (Cat. <I/131>) designation --- pmRA Proper motion in RA*cos(DE) (from AGK3) arcsec/yr pmDE Proper motion in DE (from AGK3) arcsec/yr Comments to flagged stars ID Star Designation, as in catalog.dat --- Text Text of note --- Francois Ochsenbein CDS 1998 Aug 18 UNKNOWN UNKNOWN The description above was adapted from the author's (R.A. Bartaya) manuscript. Misaligned data and erroneous positions were corrected at CDS for about 50 SAO stars, and the asterisk in ComFlag column was corrected according to the contents of notes.dat. III_112.xml Spectra of Late-Type Standard Stars in the Region 2.0-2.5 Microns 3114 III/114 Spectra of Late-Type Standards, 2.0-2.5 Microns Spectra of Late-Type Standard Stars in the Region 2.0-2.5 Microns S G Kleinmann D N B Hall Astrophys. Journ. Suppl. 62 501 1986 1986ApJS...62..501K Stars, late-type Stars, standard Spectrophotometry Spectra, infrared This catalog contains a collection of K-band spectra for 26 stars with near-solar abundances, ranging in spectral class from F8 to M7 and in luminosity from dwarfs to supergiants. The spectra cover the wavelength region from 4150 to 4950 /cm and generally exhibit a signal to noise ratio above 400. Five stars here are supergiants, 15 are giants, and six are dwarfs. Data included: observation date, starting wavenumber, wavenumber increment, scale factor of relative intensity, and offset of relative intensity.
BS_8752.fit Spectrum of BS 8752 BS_8752n.fit Noise Spectrum of BS 8752 RW_CEP.fit Spectrum of RW CEP RW_CEPn.fit Noise Spectrum of RW CEP BS_8726.fit Spectrum of BS 8726 BS_8726n.fit Noise Spectrum of BS 8726 MU_CEP.fit Spectrum of MU CEP MU_CEPn.fit Noise Spectrum of MU CEP SU_PER.fit Spectrum of SU PER SU_PERn.fit Noise Spectrum of SU PER UPS_PEG.fit Spectrum of UPS PEG UPS_PEGn.fit Noise Spectrum of UPS PEG 31_COM.fit Spectrum of 31 COM 31_COMn.fit Noise Spectrum of 31 COM 84_HER.fit Spectrum of 84 HER 84_HERn.fit Noise Spectrum of 84 HER OMI_UMA.fit Spectrum of OMIC UMA OMI_UMAn.fit Noise Spectrum of OMIC UMA EPS_VIR.fit Spectrum of EPS VIR EPS_VIRn.fit Noise Spectrum of EPS VIR IOT_CEP.fit Spectrum of IOTA CEP IOT_CEPn.fit Noise Spectrum of IOTA CEP KAP_OPH.fit Spectrum of KAP OPH KAP_OPHn.fit Noise Spectrum of KAP OPH 39_CYG.fit Spectrum of 39 CYG 39_CYGn.fit Noise Spectrum of 39 CYG GAM_DRA.fit Spectrum of GAM DRA GAM_DRAn.fit Noise Spectrum of GAM DRA GAM_SGE.fit Spectrum of GAM SGE GAM_SGEn.fit Noise Spectrum of GAM SGE 75_CYG.fit Spectrum of 75 CYG 75_CYGn.fit Noise Spectrum of 75 CYG XI_PEG.fit Spectrum of XI PEG XI_PEGn.fit Noise Spectrum of XI PEG R_LYRAE.fit Spectrum of R LYRAE R_LYRAEn.fit Noise Spectrum of R LYRAE BK_VIR.fit Spectrum of BK VIR BK_VIRn.fit Noise Spectrum of BK VIR SW_VIR.fit Spectrum of SW VIR SW_VIRn.fit Noise Spectrum of SW VIR 16CYG_A.fit Spectrum of 16 CYG A 16CYG_An.fit Noise Spectrum of 16 CYG A 16CYG_B.fit Spectrum of 16 CYG B 16CYG_Bn.fit Noise Spectrum of 16 CYG B SIG_DRA.fit Spectrum of SIG DRA SIG_DRAn.fit Noise Spectrum of SIG DRA 61CYG_A.fit Spectrum of 61 CYG A 61CYG_An.fit Noise Spectrum of 61 CYG A GL_411.fit Spectrum of GL 411 GL_411n.fit Noise Spectrum of GL 411 WOLF359.fit Spectrum of WOLF 359 WOLF359n.fit Noise Spectrum of WOLF 359 C.-H. Joseph Lyu Hughes STX/NASA 1995 Jul 13 The original ADC documentation by Kang, Y.W. and Warren, W.H. Jr. (1988) was used to create this ReadMe file. UNKNOWN UNKNOWN A magnetic tape containing the atlas Spectra of Late-Type Standard Stars in the Region 2.0-2.5 Microns was received from Dr. Susan G. Kleinmann on April 28, 1987. The tape contained 52 files one file for each signal and noise spectrum, in VAX/VMS SAVESET format. As received, each spectrum consisted of three parts: (I) the first 412 logical records contained a "big information block" (BIB) consisting of what might be termed engineering data from the Fourier transform spectrometer. This is largely redundant information from spectrum to spectrum and most of the records were actually unused; (2) a "small information block" (SIB) of two records containing in- formation pertinent to each observation, and; (3) the array of data points. Following discussions with Dr. Kleinmann, it was mutually agreed that the BIBs could be removed from the spectra, the SIBs modified slightly for easier processing, and all the spectra combined into a single file. The merging of the data simplifies the structure and is not a hindrance to processing because each spectrum contains the same number of records and can be read with a DO statement. The elimination of the redundant information also decreased the size of the catalog by a factor of 2, a definite advantage for storage requirements and dissemination. After the above modifications were made, the data were archived for distribution. The spectra are in the same order as in Table I of the source reference. III_114.xml International Ultraviolet Explorer Atlas of O-type Spectra from 1200 to 1900 A 3115 III/115 IUE Atlas of O-Type Stellar Spectra International Ultraviolet Explorer Atlas of O-type Spectra from 1200 to 1900 A N R Walborn J Nichols-Bohlin R J Panek NASA Reference Publication #1155 ??? ??? 1985 1985N86-25307.....W Stars, O Spectroscopy Spectra, ultraviolet Atlases The International Ultraviolet Explorer Atlas of O-Type Spectra From 1200 to 1900 A (Walborn et el. 1985) lists normalized fluxes and flux quality factors, splice points, and identifying information (star name/number, spectral type, SWP number, and name of the principal investigator) on 101 spectrograms of 98 O-type stars. The primary purpose of this work is to investigate the existence of systematic trends in the ultraviolet line spectra of the O stars, including the prominent stellar wind features, and the degree to which they correlate with the optical spectral classifications. A subsidiary objective is to identify ultraviolet features which may themselves prove useful as classifications criteria.
Star IDs, Spectral Types, IUE image numbers, PI names, atlas page numbers ID HD/HDE or Sanduleak (Sk) number of star --- Name Name of star --- Sp Optical spectral classification --- SWP_num SWP camera image number of observation --- PI_name Name of the IUE principal investigator --- Plate_1 First atlas plate showing spectrogram Location of of the spectrogram in the printed atlas. Each plate covers two pages in the atlas (first page covers 1200-1500 A, and the second page covers 1500-1900 A). Some spectrograms appear on more than one plate. --- Plate_2 Second atlas plate showing spectrogram --- Plate_3 Third atlas plate showing spectrogram --- Fluxes and data quality flags ID HD/HDE or Sanduleak (Sk) number of star There are 800 records for each star, and the ID appears at the beginning of each record for a given star. --- lambda Wavelength of first flux/quality pair The quoted wavelength value is the wavelength of the flux_1 and qual_1 data pair. The wavelengths for the subsequent flux/qual data pairs in the record are in increments of 0.025 nm. 0.1nm flux_1 Normalized flux at wavelength=lambda See Appendix A: "Data Preparation" for a brief description of how the normalized flux was calculated. --- qual_1 Data quality flag associated with flux_1 See Appendix A: "Data Preparation" for a brief description of how this normalized quality factor was calculated. --- flux_2 Normalized flux at wavelength=lambda+0.025 nm --- qual_2 Data quality flag associated with flux_2 --- flux_3 Normalized flux at wavelength=lambda+0.050 nm --- qual_3 Data quality flag associated with flux_3 --- flux_4 Normalized flux at wavelength lambda+0.075 nm --- qual_4 Data quality flag associated with flux_4 --- Splice points of spectra ID HD/HDE or Sanduleak (Sk) number of star There are 13 records for each star, and the ID appears at the beginning of each record for a given star. --- splice1 First splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice2 Second splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice3 Third splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice4 Fourth splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice5 Fifth splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice6 Sixth splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice7 Seventh splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice8 Eighth splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm Joel W. Parker GSFC/Code 680 1995 Aug 07 UNKNOWN UNKNOWN A. Data Preparation: This section briefly describes the steps involved in selecting and processing the data comprising this atlas. The following description was extracted from an edited version of Walborn et al. (1995). A.1 Selection Approximately 200 O stars have short-wavelength, high-resolution data in the IUE archive. 120 of these were examined for possible inclusion in the atlas. The primary selection criterion was the availability of homogeneous optical spectral classifications by Walborn (1972 AJ 77, 312; 1973 AJ 78, 1067). In general, known interacting binaries and very rapid rotators were avoided, but a number of peculiar objects and categories which have been well described optically were specifically included. A.2 Processing The IUE Spectral Image Processing System (IUESIPS) data were retrieved from the IUE data archive. Each gross spectrum included samples of the observed signal along each echelle order, integrated along a pseudo-slit; and a corresponding sample of the interorder background. Sample wavelength and a data quality indicator were also included. Processing then proceeded through the following steps: 1. The background was smoothed and subtracted from the on-order signal to yield the net spectrum. 2. A "ripple" correction was applied to adjust for systematic variation along each order caused by the varying sensitivity of the echelle grating. Overlap among adjacent orders [was] discarded beyond the wavelengths at which which the sensitivities [were] equal. These points of overlap are listed in the second file. The spectrum was then resampled to 0.25 A resolution: Each original sample was considered an estimate of the flux averaged over a bin whose width was equal to the spacing between the adjacent points. Each new sample was computed as a weighted average of the original samples; the weight of each original sample is equal to the fraction of its bin which falls within the 0.25 A window centered on the new wavelength point. However, the weight is zero for any original point for which the IUESIPS quality factor indicated contamination by a camera reseau, saturation of the vidicon camera, or a particle radiation hit. The new sample points were spaced evenly at 0.25 A intervals from 1150 A to 1950 A. For each new sample point, a quality factor was computed as the sum of the weights for the original samples contributing to the new point. This quality factor ranges from about 6 at 1200 A (where there is no effect of a reseau, etc.) to about 4 at 1800 A for IUESIPS processing at GSFC before November 1981. With the newer version of IUESIPS, this factor is roughly doubled due to the finer wavelength sampling of the spectrum. 3. The resampled spectrum was then rescaled in order to locate the stellar continuum at an approximately uniform level: This ... was performed interactively ... by identifying about a dozen "continuum" points spaced along the interval 1150-1950 A. Then, the flux was divided by a cubic spline interpolated through these points. The intention here was not to precisely define a stellar continuum; it was simply to place the spectrum onto a convenient scale for plotting over the full spectral range. The renormalization function usually showed a broad hump between 1400 and 1600 A. It is unclear whether this represents a rise in the instrument sensitivity near 1500 A or an effect of blended spectral absorption features near 1400 and 1600 A. Similarly, the data quality factor was normalized to remove the effect of the decreasing spectral dispersion toward longer wavelengths, which causes the number of original samples within a 0.25 A window to decrease. Narrow positive spikes in the flux data due to particle radiation hits and the geocoronal Lyman alpha emission were eliminated manually. In addition, the catalog authors note the following: Small deviations from unity in the data quality factor occur where a few of the original sample points in the 0.25 A resample window were contaminated by a reseau. Large deviations from unity occur where most or all of the points were affected by a reseau. In many cases, no effect of the reseau is apparent in the stellar spectrum; this occurs when the reseau falls close to but not precisely onto the stellar spectrum, and the interorder background is weak. III_115.xml Spectrophotometric Standards 3116 III/116 Spectrophotometric Standards Spectrophotometric Standards P Massey K Strobel J V Barnes E Anderson Astrophys. J. 328 315 1988 1988ApJ...328..315M Spectrophotometry Stars, standard The stellar magnitude system is based on the brightness of Vega at each wavelength. Vega, itself, has been compared accurately with laboratory standards. Unfortunately, Vega is much too bright to be observed under the same conditions with most stars of interest. Hence, various investigators have compared carefully with Vega and a few other primary standards somewhat fainter stars to be used as secondary standards. In addition, several much fainter stars have been used as tertiary standards with lower accuracy. With the common use of linear detectors and large telescopes, it has become important to provide spectrophotometric standards for a range of magnitudes including quite faint stars. The planning for the Hubble Space Telescope increased the necessity for fainter standards. Moreover, both the IUE and the HST require that the standards be established at the shortest wavelength reliably accessible from the ground so that ultraviolet spectrophotometry can be tied to visual spectrophotometry accurately. Investigators at Kitt Peak National Observatory have pursued a lengthy program to provide both more accurate spectrophotometry of faint stars and a dense distribution of the wavelengths at which the fluxes are measured. The close spacing of points is essential to place the fairly short stretches of a high resolution spectrum available with a solid state detector on a standard system. The present compilation provides improved data for nine stars previously observed by Stone (1977) or Oke (1974) and spectro- photometry of 16 new standards, eight of which are fainter than 14.0 mag. To provide red standards and still avoid stars with numerous spectral lines, a highly reddened O5 star and two substantially reddened (but bright) O5 stars are included. The observations were all referenced to either BD+28 4211 or Feige 34. For four stars in common, comparison with the data from Stone indicates that the calibration of the standard stars is good to about 0.03 mag. The internal accuracy of the data for the individual stars is substantially higher. The measurements are on the Hayes-Latham system. Table 1 describes the stars. It is identical to Table 1 in the source reference except that V has been omitted. The number of observations per star ranges from 3 to 29, but not all observations were made under photometric conditions. Only one observation of Feige 110 was made under photometric conditions. For PG 0205+134, PG 0310+149, PG 0939+262, PG 1121+145, and PG 1545+035, only two measurements were made under photometric conditions. The magnitudes for HZ44 show a large scatter within the 29 measurements. Fig. 1, also from the source reference, provides finding fields for all stars except for the two brightest. Observers at the National Optical Astronomy Observatories have provided spectrophotometry for 25 stars in the visual magnitude range 7.5 to 16.6. This document describes the machine-readable version of their results as received from P. Massey. The magnitudes are on the Hayes-Latham system and cover the wavelength range from 3200 to 8100 angstroms at approximately two angstrom intervals.
List of stars with spectrophotometry File Name of the file which contains the spectrophotometry --- Star Name of the star --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec SpType Spectral type --- m5666 Magnitude number=1 All magnitudes are m_5556 except for PG 0934+554 for which V is given. For PG 0205+134, PG 0216+032, PG 0310+149, PG 0939+262, and PG 1708+602, the g-v indices of Green, Schmidt, and Liebert have been substituted for B-V. mag B-V colour mag Notes Notes concerning the star --- Spectrum of PG 0205+134 Spectrum of PG 0216+032 Spectrum of PG 0310+149 Spectrum of HZ 14 Spectrum of G 191B2B Spectrum of Hiltner 600 Spectrum of PG 0823+546 Spectrum of PG 0846+249 Spectrum of PG 0934+554 Spectrum of PG 0939+262 Spectrum of Feige 34 Spectrum of PG 1121+145 Spectrum of GD 140 Spectrum of EG 81 Spectrum of Feige 66 Spectrum of Feige 67 Spectrum of HZ 44 Spectrum of PG 1545+035 Spectrum of PG 1708+602 Spectrum of HD 192281 Spectrum of Cyg OB2 No.9 Spectrum of Wolf 1346 Spectrum of BD +28 4211 Spectrum of HD 217086 Spectrum of Feige 110 Lambda Wavelength (Angatroems) 0.1nm m(Lambda) Magnitude on the Hayes-Latham system mag Francois Ochsenbein CDS 1995 Sep 11 We thank Dr. Massey for forwarding to us the Spectrophotometric Data in easily machine-readable form and for the accompanying reprint. UNKNOWN UNKNOWN * September 1991 at ADC: The Spectrophotometric Standards catalog was received from Dr. Massey in August 1987 in 25 machine-readable files, one for each star. These files have been concatenated into a single file. The documentation was written by Nancy G. Roman, Doc. No. NSSDC/WDC-A-R&S 91-09 Files on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM, directory /spectro/spstd * 11-Sep-1995: documentation standardized; individual files have been recreated to allow standard conversions into FITS of each spectrum. III_116.xml G.P. Kuiper's Spectral Classifications of Proper-Motion Stars 3119 III/119 Kuiper's Spectral Classifications Prop-Mot Stars G.P. Kuiper's Spectral Classifications of Proper-Motion Stars W P Bidelman Astrophys. J. Suppl. 59 197 1985 1985ApJS...59..197B Spectral types This catalogue lists the spectral classifications of over 3200 stars, mainly of large proper motion, observed and classified by the late Dr. G.P. Kuiper during the years 1937-1944 at the Yerkes and McDonald Observatories. While Kuiper himself published many of his types, and while improved classifications are now available for many of these stars, much of value remains: for a great many of the objects no other spectral data exist.
LTT Stars LTT LTT number The user is referred to Luyten (1957, 1961, 1962) for coordinates, proper motions and other details on the stars contained in lttstars.dat. --- n_LTT Suffix to LTT number = = two stars are the same / = double with two components listed --- name Star name --- V Photoelectric V magnitude Photoelectric V magnitude is largely taken from the extensive compilation by Jaschek et al. (1972), but includes many from other sources. For variable stars, magnitude data are taken from the GCVS and its supplements. Magnitudes listed with a following "v" are visual or photovisual magnitudes taken from Kuiper's original file cards. For many of the fainter stars these are no doubt eye estimates at the telescope. mag Sp Spectral type Luminosity classes were not usually given by Kuiper. The letter "f" following a spectral type indicates that the lines appeared weak. --- note Individual notes --- Additional Stars name Star name --- RAh Right Ascension (1900) hours h RAm Right Ascension (1900) minutes min DE- Declination (1900) sign --- DEd Declination (1900) degrees deg DEm Declination (1900) arcminutes arcmin V Photoelectric V magnitude Photoelectric V magnitude is largely taken from the extensive compilation by Jaschek et al. (1972), but includes many from other sources. For variable stars, magnitude data are taken from the GCVS and its supplements. Magnitudes listed with a following "v" are visual or photovisual magnitudes taken from Kuiper's original file cards. For many of the fainter stars these are no doubt eye estimates at the telescope. mag Sp Spectral type Luminosity classes were not usually given by Kuiper. The letter "f" following a spectral type indicates that the lines appeared weak. : = uncertain :: = very uncertain --- note Individual notes --- Julie Anne Watko SSDOO/ADC 1996 Aug 20 III_119.xml Catalogue of Stars with Ca II H and K Emissions 3120 III/120 Stars with Ca II H and K Emissions Catalogue of Stars with Ca II H and K Emissions R Glebocki G Musielak A Stawikowski Acta Astron. 30 453 1980 1980AcA....30..453G Stars, emission Intensities and widths of emission cores of H and K lines from the literature are presented for over 1400 stars of spectral types F, G, K and M.
Emission data from the literature HD/BD Identification Number: HD or BD --- Sp Spectral Type --- V Apparent Visual Magnitude mag B-V Color Index mag IHK Intensity of K emission Intensity of K emission in scales originally used by authors. --- n_IHK Suffix to IHK This field may contain a second decimal place or the exponential part of an intensity expressed in scientific notation. --- r_IHK Source of IHK 1. Wilson O.C. 1976 2. Wilson O.C. 1967 3. Wilson O.C. & Bappu M.K.V. 1957 4. Warner B. 1969 5. Kraft R.P., Preston G.W. & Wolff S.C. 1964 6. Wilson O.C. 1963 7. Wilson O.C. 1962 8. Herbig G.H. 1965 9. Wilson O.C. & Wolley R. 1970 10. Wilson O.C. 1959 11. Stencel R.E. 1977 12. Young A. & Koniges A. 1977 13. Glebocki and Stawikowski (unpublished) 14. Linsky J.L., Worden S.P., McClintock W. & Robertson R.M. 1979 For references 1, 2, 3, 5, 6, 7, 8, 10, 11, 13, 14, intensities are in Wilson's scale 0-5; for reference 4 intensities are in scale 0-8 and for reference 9 intensities are in scale (-5)-(+6). Young and Koniges (reference 12) did not make intensity estimates on a scale consistent with Wilson's. IHK values for this reference are given in scientific notation. --- W0 Width of K Emission Width of K emission as defined in the following formula: W0=log((dl/l)*c) where dl is the wavelength difference on both edges of emission core --- r_W0 Source of W0 1. Wilson O.C. 1976 2. Wilson O.C. 1967 3. Wilson O.C. & Bappu M.K.V. 1957 4. Warner B. 1969 5. Kraft R.P., Preston G.W. & Wolff S.C. 1964 6. Wilson O.C. 1963 7. Wilson O.C. 1962 8. Herbig G.H. 1965 9. Wilson O.C. & Wolley R. 1970 10. Wilson O.C. 1959 11. Stencel R.E. 1977 12. Young A. & Koniges A. 1977 13. Glebocki and Stawikowski (unpublished) 14. Linsky J.L., Worden S.P., McClintock W. & Robertson R.M. 1979 For references 1, 2, 3, 5, 6, 7, 8, 10, 11, 13, 14, intensities are in Wilson's scale 0-5; for reference 4 intensities are in scale 0-8 and for reference 9 intensities are in scale (-5)-(+6). Young and Koniges (reference 12) did not make intensity estimates on a scale consistent with Wilson's. IHK values for this reference are given in scientific notation. --- rem Remarks 1 = value in IHK represents equivalent width in mA --- Nancy Grace Roman, Julie Anne Watko SSDOO/ADC 1996 Aug 12 III_120.xml Catalogue of Stellar Abundances 3121 III/121 Stellar Abundances Catalogue of Stellar Abundances A Marecki J Strobel A Strobel Osservatorio Astronomico di Torino ??? ??? 1986 1986 Abundances The catalog consists of two parts - the first contains the published abundances, the second gives the bibliographic references to the data. In addition to the abundance of individual elements the values of the metal-to-hydrogen parameter in the form (M/H) are also given. For each abundance a numerical code for the bibliographic reference is added.
Catalog Data Name Identification of the star --- Seq Running number for a star --- Element Symbol of element (M/H denotes metallicity) --- Unit Code for original abundance form Code of the form of the abundance determination as cited in the original literature: 1 = (Nel/Nel) relative to the reference star 2 = log(Nel/Nel) relative to the reference star 3 = log(Nel) for log.H = 12 or log.H = 24 4 = (Nel/Nel) 5 = other form --- RefElem Name of reference element (H12 for log.H=12, H24 for log.H=24, Fe, etc...) --- n_Stand Code for reference object Code for the reference object relative to which the abundance is determined: O = the Sun S = the star other than the Sun B = other reference "object" like average value of the abundance of a given element for a group of stars --- Stand Name of the standard (reference) star or object --- Method Code for method of abundance determination Code for the method of abundance determination: H = based on spectra of high dispersion (up to 20 Angstrom/mm) S = based on spectra of small dispersion P = based on photographic photometry E = based on photoelectric photometry --- Abun Value of the abundance determination is cited in the publication --- e_Abun Error of the abundance determination as cited in the publication --- Ref Bibliographic reference; the list of references is not available. --- Com Comments --- James E. Gass SSDOO/ADC 1997 Sep 09 III_121.xml The Interstellar 217-nm Band: A Third Catalogue of Equivalent Widths 3122 III/122 Interstellar 217-nm Band: Equivalent Widths 3 The Interstellar 217-nm Band: A Third Catalogue of Equivalent Widths C Friedemann U K Roder Astron. Nachr. 308 41 1987 1987AN....308...41F Equivalent widths Interstellar medium Using the data obtained with the ultraviolet photometer in the Astronomical Netherlands Satellite, the equivalent widths of the interstellar 217 nm band as well as other parameters characterizing the behavior of the continuous interstellar extinction in the wavelength region of the band have been derived for 790 O, B stars with color excesses E(B-V) >= 0.4 mag.
Equivalent width data ID HD or BD Identification HD is right justified to byte 6. BD zone appears in bytes 1-3. BD number is right justified to byte 9. --- E(B-V) E(B-V) Color excess mag alpha {alpha} parameter --- beta {beta} parameter --- gamma {gamma} parameter --- W Equivalent width in Angstroms 0.1nm S2200 Standard deviation (Wesselius et al. 1982) Standard deviation in 0.001mag in the 2200 A band according to Wesselius et al. (1982) 10-3mag N Number of separate observations (Ibid.) --- rem Remarks 3 = common star with an entry in the catalog compiled by Dorschner et al. (1984) 4 = at least two stars are present within one arcminute of the pointing position 5 = ultraviolet results indicate variability 50 = suspected variable 6 = equivalent width W deviates two to three times the standard deviation of the mean relation W ~ E(B-V) 70 = possibly a deviating extinction law 8 = lying in a cluster that probably affects the ultraviolet data 9 = equivalent width W deviates at least three times the standard deviation from the mean relation W ~ E(B-V) --- Julie Anne Watko SSDOO/ADC 1996 Aug 15 UNKNOWN UNKNOWN supersedes III/95 III_122.xml Dwarf K And M Stars of small proper motion found in a Large Spectroscopic Survey 3123A III/123A Dwarf K and M stars of small proper motion Dwarf K And M Stars of small proper motion found in a Large Spectroscopic Survey C B Stephenson Astron. J. 91 144 1986 1986AJ.....91..144S Stars, dwarfs Stars, late-type More than 2000 candidates for K and M dwarf status, generally having proper motions that are either unknown or less than 0.2" per annum, have been identified in an objective-prism survey covering the entire sky north of declination -25deg and more than 10deg from the galactic plane. More than 95% have no previous indication that they are dwarfs. Several dozen appear to be visual double stars.
The Catalogue of 2201 stars Star Star number --- n_Star The asterisk indicates a note in file 'notes' --- RAh Right ascension 1900 (hours) h RAm Right ascension 1900 (minutes) min RAs Right ascension 1900 (seconds) s DE- Declination 1900 (sign) --- DEd Declination 1900 (degrees) deg DEm Declination 1900 (minutes) arcmin DEs Declination 1900 (seconds) arcsec Pmag Stellar photographic magnitude mag Sp Spectral type --- Names Names from other lists --- Francois Ochsenbein, Joseph Florsch CDS 1995 Mar 15 UNKNOWN UNKNOWN * Keypunched at CDS * 15-Mar-1995: added file 'notes', the '*' flag in file 'catalog'; several clerical errors corrected in the course of the standardisation. III_123A.xml Spectrophotometry of bright F, G, K and M-type stars. 60 Southern and Equatorial stars 3124 III/124 Spectrophotometry of 60 stars Spectrophotometry of bright F, G, K and M-type stars. 60 Southern and Equatorial stars R Kiehling Astron. Astrophys. Suppl. Ser. 69 465 1987 1987A&AS...69..465K III/88 : Stellar Spectrophotometric Atlas (Gunn+ 1983) III/92 : A Library of Stellar Spectra (Jacoby+ 1984) III/124 : Spectrophotometry of 60 stars (Kiehling, 1987) III/166 : A New Library of Optical Spectra (Silva+ 1992) III/196 : Near-IR stellar spectra from 1.428 to 2.5 um (Lancon+ 1996) J/PASP/110/863 : A Stellar Spectral Flux Library 1150-25000{AA} (Pickles 1998) Spectrophotometry Spectral energy distributions were photoelectrically measured from 320 to 860 nm with a resolution of 1 nm in equidistant steps of 1 nm for 60 bright southern and equatorial stars of intermediate and late spectral types for all luminosity classes. Flux curves for individual stars are plotted with a resolution of 1 nm and tabulated in steps of 5 nm. Typical internal mean errors of fluxes measured in different nights are less than 0.02mag in the spectral range from 400 nm to 860 nm, and rise to a maximum of about 0.05mag for wavelengths below 400 nm.
The 60 stars Name Identification of stars --- RAh Right Ascension J2000 (hours) (from SIMBAD) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) (from SIMBAD) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec F(555nm) Flux at 555 nm (unspecified units) --- Sp MK spectral type --- Vmag Johnson's V magnitude mag The spectra lambda Wavelength nm m(HR1325) Normalized mag. HR 1325 number=1 unmeasured magnitudes are set to 99.999 mag m(HR1457) Normalized mag. HR 1457 number=1 unmeasured magnitudes are set to 99.999 mag m(HR1654) Normalized mag. HR 1654 number=1 unmeasured magnitudes are set to 99.999 mag m(HR1829) Normalized mag. HR 1829 number=1 unmeasured magnitudes are set to 99.999 mag m(HR1865) Normalized mag. HR 1865 number=1 unmeasured magnitudes are set to 99.999 mag m(HR1983) Normalized mag. HR 1983 number=1 unmeasured magnitudes are set to 99.999 mag m(HR2061) Normalized mag. HR 2061 number=1 unmeasured magnitudes are set to 99.999 mag m(HR2085) Normalized mag. HR 2085 number=1 unmeasured magnitudes are set to 99.999 mag m(HR2326) Normalized mag. HR 2326 number=1 unmeasured magnitudes are set to 99.999 mag m(HR2580) Normalized mag. HR 2580 number=1 unmeasured magnitudes are set to 99.999 mag m(HR2646) Normalized mag. HR 2646 number=1 unmeasured magnitudes are set to 99.999 mag m(HR2693) Normalized mag. HR 2693 number=1 unmeasured magnitudes are set to 99.999 mag m(HR2943) Normalized mag. HR 2943 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3043) Normalized mag. HR 3043 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3153) Normalized mag. HR 3153 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3185) Normalized mag. HR 3185 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3188) Normalized mag. HR 3188 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3249) Normalized mag. HR 3249 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3438) Normalized mag. HR 3438 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3547) Normalized mag. HR 3547 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3634) Normalized mag. HR 3634 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3684) Normalized mag. HR 3684 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3748) Normalized mag. HR 3748 number=1 unmeasured magnitudes are set to 99.999 mag m(HR3873) Normalized mag. HR 3873 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4050) Normalized mag. HR 4050 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4110) Normalized mag. HR 4110 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4114) Normalized mag. HR 4114 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4159) Normalized mag. HR 4159 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4362) Normalized mag. HR 4362 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4441) Normalized mag. HR 4441 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4511) Normalized mag. HR 4511 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4517) Normalized mag. HR 4517 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4523) Normalized mag. HR 4523 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4532) Normalized mag. HR 4532 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4540) Normalized mag. HR 4540 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4616) Normalized mag. HR 4616 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4630) Normalized mag. HR 4630 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4763) Normalized mag. HR 4763 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4786) Normalized mag. HR 4786 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4910) Normalized mag. HR 4910 number=1 unmeasured magnitudes are set to 99.999 mag m(HR4932) Normalized mag. HR 4932 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5019) Normalized mag. HR 5019 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5072) Normalized mag. HR 5072 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5192) Normalized mag. HR 5192 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5235) Normalized mag. HR 5235 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5261) Normalized mag. HR 5261 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5288) Normalized mag. HR 5288 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5340) Normalized mag. HR 5340 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5459) Normalized mag. HR 5459 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5460) Normalized mag. HR 5460 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5854) Normalized mag. HR 5854 number=1 unmeasured magnitudes are set to 99.999 mag m(HR5868) Normalized mag. HR 5868 number=1 unmeasured magnitudes are set to 99.999 mag m(HR6020) Normalized mag. HR 6020 number=1 unmeasured magnitudes are set to 99.999 mag m(HR6030) Normalized mag. HR 6030 number=1 unmeasured magnitudes are set to 99.999 mag m(HR6056) Normalized mag. HR 6056 number=1 unmeasured magnitudes are set to 99.999 mag m(HR6102) Normalized mag. HR 6102 number=1 unmeasured magnitudes are set to 99.999 mag m(HR6159) Normalized mag. HR 6159 number=1 unmeasured magnitudes are set to 99.999 mag m(HR6406) Normalized mag. HR 6406 number=1 unmeasured magnitudes are set to 99.999 mag m(HD156026) Normalized mag. HD 156026 number=1 unmeasured magnitudes are set to 99.999 mag m(HR6623) Normalized mag. HR 6623 number=1 unmeasured magnitudes are set to 99.999 mag Joseph Florsch, Francois Ochsenbein CDS 1998 Oct 06 UNKNOWN UNKNOWN * 21-Nov-1994: first description of catalog (Joseph Florsch, CDS) * 06-Oct-1998: positions of stars added (from SIMBAD) III_124.xml Stellar Spectrophotometric Catalogue 3126 III/126 Spectrophotometry of 1588 stars Stellar Spectrophotometric Catalogue V I Burnashev Abastumanskaya Astrofiz. Obs. Bull. 59 83 1985 1985AbaOB..59...83B Spectrophotometry The present catalogue contains 2238 energy distribution data for 1588 objects in the spectral region 320-735nm by steps of 2.5nm. It is based on the following spectrophotometric catalogues: Kharitonov et al. (1), Alekseev et al. (the "Chilean Catalogue") (2), Willstrop (3), Glushneva et al. (the "Moscow Catalogue") (4,5,6), Burnashev's observations of stars obtained at the Crimean Astrophysical Observatory. Comparison of these catalogues and their reductions to the uniform spectrophotometric system has been carried out by Burnashev (7). The catalogue is divided in three parts: 1) Part 1 contains the data published in the catalogues by Kharitonov (1), Glushneva (4,5,6) and Willstrop(3). 2) Part 2 contains the data (and their r.m.s) of the "Chilean Catalogue" (Alekseev et al.(2)) and Burnashev's observations of some stars, obtained at the Crimean Astrophysical Observatory during 1974-1982. The observations of some variables, obtained in Chile, Are also presented. This part contains also tables of the Hydrogen continuum radiation for several temperatures (5000; 10000;15000;20000;40000;80000 K) according to Boyarchuk et al.(9), which may be useful for the analysis of the spectra of some variables. 3) Part 3 contains data of Parts 1 and 2 reduced to the uniform spectrophotometric system of the "Chilean Catalogue" in the range 320-735nm. The absolute calibration based on energy distribution of the primary standard Alpha Lyrae, according to Kharitonov (10), being the mean of the absolute calibrations of Kharitonov et al.(11), Hayes and Latham (12), Tug et al.(13).
Spectrophotometry by Kharitonov, Glushneva, Willstrop Spectrophotometry reduced to "Chilean System" Name Basic names of star number=1 the names include the BS (Bright Star catalogue <V/50>) or HS (Henry Draper, catalog <III/135>), followed by the Bayer/Flamsteed name. The Pleiades stars are numbered from Herzsprung's (8) catalogue. --- Vmag Visual magnitude (with annotations) mag SpType Spectral classification --- Date of observation, when known --- Origin of data number=2 the origin is coded as: (blank) is Kharitonov et al., ref. (1) CHL = "Chilean Catalogue", ref. (2) CRM = Burnashev's observations at the Crimean Observatory MSK = Glushneva, ref. (4) WIL = Wilstrop, ref. (3) --- Nobs Number of observations --- lambda1 Bluest wavelength 0.1nm log(E) Logarithm of energy (in erg/s/cm2/cm) mW/m2/cm Chilean Catalogue by Alekseev et al. Name Basic names of star, see note (1) above --- Vmag Visual magnitude (with annotations) mag SpType Spectral classification --- Date of observation, when known --- Origin of data, see note (2) above --- Nobs Number of observations --- lambda1 Bluest wavelength 0.1nm log(E) Logarithm of energy (in erg/s/cm2/cm) mW/m2/cm List of stars observed Name Basic names of star, see note (1) above --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec SpType Spectral classification --- Francois Ochsenbein CDS 1996 Apr 15 UNKNOWN UNKNOWN The data on magnetic tape were received from the Moscow Data Center in 1987. The file "stars", which contains the list of the stars contained in the catalogue together with its position, was added at CDS, using the SIMBAD data-base. III_126.xml Radial Velocities of Bright Southern Stars I 3127 III/127 Radial Velocities of Bright Southern Stars Radial Velocities of Bright Southern Stars I J Andersen B Nordstroem Astron. Astrophys. Suppl. Ser. 52 471 1983 1983A&AS...52..471A Radial Velocities of Bright Southern Stars I J Andersen B Nordstroem Astron. Astrophys. Suppl. Ser. 52 479 1983 1983A&AS...52..479A Radial Velocities of Bright Southern Stars I B Nordstroem J Andersen Astron. Astrophys. Suppl. Ser. 61 53 1985 1985A&AS...61...53N Radial velocities Stars, bright Radial Velocities of Bright Southern Stars is the result of an effort to determine radial velocities for those southern stars in the "Bright Star Catalogue" with no previously published radial velocity. This version of the catalog combines three lists of data published separately during 1983-85, the first for B-type stars, the second for late-type stars, and the last for A- and F-type stars. J. Andersen notes the following in a 1987 private communication: "In order to make the 1982 edition of the "Bright Star Catalogue" as complete as possible, preliminary or even incomplete data for many stars in this catalogue were provided in advance of publication. The present catalogue presents the final values, which should supersede (not be averaged with!) those given in the Bright Star Catalogue." See Andersen & Nordstroem (1983) for a detailed description of the method employed throughout the entire observation program.
The Catalogue HD HD number --- HDsuffix HD suffix --- HR Bright Star Catalogue number --- FK4 FK4 / FK4 Supp. number --- V Visual magnitude Visual magnitude from Hoffleit (1964) or Olsen (1977) mag u_V Uncertainty flag (:) on V magnitude --- r_Sp Reference of spectral class References of Spectral Class - =00= Hoffleit D., "Catalogue of Bright Stars", 3rd ed. (1964), 4th ed. (1982) =01= Houk N., Cowley A.P., 1975, Michigan Catalogue of Spectral Types for HD stars, Vol. 1 =02= Kennedy M.P., 1977, MK Catalogue (CDS) =03= Cowley A.P., 1976, PASP 88, 95 =04= Harlan E.A., 1974, AJ 79, 682 =05= Cowley A.P., Fraquelli D., 1974, PASP 86, 70 =06= Hube D.P., 1970, Mem. RAS 72, 233 =07= Abt H.A., Levato H., 1977, PASP 89, 797 =08= Malaroda S., 1975, AJ 80, 637 =09= Houk N., 1978, Michigan Catalogue of Spectral Types for HD stars, Vol. 2 =10= Andersen J., Nordstroem B., 1977, A&AS 29, 309 =11= Andersen J., Nordstroem B., 1978, BICDS 15, 39 =12= Cowley A.P., Bidelman W.P., 1979, PASP 91, 83 =13= Houk N., 1982, Michigan Catalogue of Spectral Types for HD stars, Vol.3 --- Sp MK spectral class --- RV Radial Velocity of the primary stellar comp. Radial Velocity of the primary stellar component. Any secondary components are indicated by a note in file "notes" (see Remarks field) km/s u_RV Uncertainty flag (:) on RV --- e_RV Mean error on RV km/s u_e_RV Uncertainty flag (:) on e_RV --- o_RV Number of plates measured in determining RV Number of plates measured in determining the radial velocity and error --- RVvel Velocity Variability parameter This parameter "measures the ratio between the observed plate-to-plate scatter for a given star and the scatter expected for a constant star measured with the same uncertainty" varVel=1.75 is considered the lower limit for possible variability in velocity, and varVel=2.5 the lower limit for certain variability. See Andersen & Nordstroem (1983) --- RV(HK) Velocity of interstellar H and K lines Velocity of interstellar H and K lines when measured separately km/s e_RV(HK) Mean error on RV(H+K) km/s RotClass Rotation Class The rotation class has the values: =0= v.sin(i) < 15km/s =1= 15 < v.sin(i) < 50km/s =2= 50 < v.sin(i) < 100km/s =3= 100 < v.sin(i) < 175km/s =4= 175 < v.sin(i) < 250km/s =5= v.sin(i) > 250km/s --- rem remarks, binarity, variability Remarks are indicated by one or more of the following "words": REM Remark in file "notes" SB2 Double-line spectroscopic binary SB3 Triple-line spectroscopic binary VAR Certain variability VAR? Possible variability --- The Observations HD HD number --- HDsuffix HD suffix --- JD Julian date of observation d Weight of the plate --- RV1 Radial velocity of the primary km/s e_RV1 Mean error on RV1 km/s Num1 Number of lines measured to determine RV1 --- RV2 RV of the secondary or emission component Radial velocity of either the secondary in SB2 (indicated by "SB2" in the "Remarks" field of file "results"), or the emission component. km/s e_RV2 Mean error on RV2 km/s Num2 Number of lines measured to determine RV2 --- RV3 Radial velocity of the third or shell Radial velocity of either the third star in SB3 (indicated by "SB3 in the "Remarks" field of file "results"), or the shell component. km/s e_RV3 Mean error on RV3 km/s Num3 Number of lines measured to determine RV3 --- Remarks HD HD number HD number and suffix; when these fields are blank, it is a continuation of the previous line. --- HDsuffix HD suffix --- rem remark Numbers in parentheses correspond to the references listed in "Note on r_Sp" above. --- C.-H. Joseph Lyu, Paul Kuin NASA ADC F. Ochsenbein CDS 1997 Jan 08 This description was adapted from the original ADC documentation "Documentation for Machine-Readable Version" by Anne C. Raugh. The full JD observation date has been inserted in the "obs" file at CDS. The ReadMe documentation was prepared by F. Ochsenbein and J. Lyu. III_127.xml Atlas of the Wavelength Dependence of Ultraviolet Extinction in the Galaxy 3130 III/130 Wavelength Dependence of Galactic UV Extinction Atlas of the Wavelength Dependence of Ultraviolet Extinction in the Galaxy S Aiello B Barsella G Chlewicki J M Greenberg P Patriarchi M Perinotto Astron. Astrophys. Suppl. Ser. 73 195-208 1988 1988A&AS...73..195A Extinction Spectra, ultraviolet A collection of data for 115 extinction curves derived from low-dispersion IUE spectra are presented with normalization to E(B-V)=1. The electronic Atlas of Extinctions contains the list of the stars used, their association membership, and the normalized extinctions for 88 wavelength values between 1260 and 3000 Angstroems.
The Atlas of Extinction data Seq Running number --- Name Star name --- Assoc Association name --- RAh Right Ascension 2000 (hours) the positions differ from those printed in table4 (they were extracted from the SIMBAD data-base in April 1998) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec E3000 Extinction ratio E(300nm-V)/E(B-V) --- E2980 Extinction ratio E(298nm-V)/E(B-V) --- E2960 Extinction ratio E(296nm-V)/E(B-V) --- E2940 Extinction ratio E(294nm-V)/E(B-V) --- E2920 Extinction ratio E(292nm-V)/E(B-V) --- E2900 Extinction ratio E(290nm-V)/E(B-V) --- E2880 Extinction ratio E(288nm-V)/E(B-V) --- E2860 Extinction ratio E(286nm-V)/E(B-V) --- E2840 Extinction ratio E(284nm-V)/E(B-V) --- E2820 Extinction ratio E(282nm-V)/E(B-V) --- E2800 Extinction ratio E(280nm-V)/E(B-V) --- E2780 Extinction ratio E(278nm-V)/E(B-V) --- E2760 Extinction ratio E(276nm-V)/E(B-V) --- E2740 Extinction ratio E(274nm-V)/E(B-V) --- E2720 Extinction ratio E(272nm-V)/E(B-V) --- E2700 Extinction ratio E(270nm-V)/E(B-V) --- E2680 Extinction ratio E(268nm-V)/E(B-V) --- E2660 Extinction ratio E(266nm-V)/E(B-V) --- E2640 Extinction ratio E(264nm-V)/E(B-V) --- E2620 Extinction ratio E(262nm-V)/E(B-V) --- E2600 Extinction ratio E(260nm-V)/E(B-V) --- E2580 Extinction ratio E(258nm-V)/E(B-V) --- E2560 Extinction ratio E(256nm-V)/E(B-V) --- E2540 Extinction ratio E(254nm-V)/E(B-V) --- E2520 Extinction ratio E(252nm-V)/E(B-V) --- E2500 Extinction ratio E(250nm-V)/E(B-V) --- E2480 Extinction ratio E(248nm-V)/E(B-V) --- E2460 Extinction ratio E(246nm-V)/E(B-V) --- E2440 Extinction ratio E(244nm-V)/E(B-V) --- E2420 Extinction ratio E(242nm-V)/E(B-V) --- E2400 Extinction ratio E(240nm-V)/E(B-V) --- E2380 Extinction ratio E(238nm-V)/E(B-V) --- E2360 Extinction ratio E(236nm-V)/E(B-V) --- E2340 Extinction ratio E(234nm-V)/E(B-V) --- E2320 Extinction ratio E(232nm-V)/E(B-V) --- E2300 Extinction ratio E(230nm-V)/E(B-V) --- E2280 Extinction ratio E(228nm-V)/E(B-V) --- E2260 Extinction ratio E(226nm-V)/E(B-V) --- E2240 Extinction ratio E(224nm-V)/E(B-V) --- E2220 Extinction ratio E(222nm-V)/E(B-V) --- E2200 Extinction ratio E(220nm-V)/E(B-V) --- E2180 Extinction ratio E(218nm-V)/E(B-V) --- E2160 Extinction ratio E(216nm-V)/E(B-V) --- E2140 Extinction ratio E(214nm-V)/E(B-V) --- E2120 Extinction ratio E(212nm-V)/E(B-V) --- E2100 Extinction ratio E(210nm-V)/E(B-V) --- E2080 Extinction ratio E(208nm-V)/E(B-V) --- E2060 Extinction ratio E(206nm-V)/E(B-V) --- E2040 Extinction ratio E(204nm-V)/E(B-V) --- E2020 Extinction ratio E(202nm-V)/E(B-V) --- E2000 Extinction ratio E(200nm-V)/E(B-V) --- E1980 Extinction ratio E(198nm-V)/E(B-V) --- E1960 Extinction ratio E(196nm-V)/E(B-V) --- E1940 Extinction ratio E(194nm-V)/E(B-V) --- E1920 Extinction ratio E(192nm-V)/E(B-V) --- E1900 Extinction ratio E(190nm-V)/E(B-V) --- E1880 Extinction ratio E(188nm-V)/E(B-V) --- E1860 Extinction ratio E(186nm-V)/E(B-V) --- E1840 Extinction ratio E(184nm-V)/E(B-V) --- E1820 Extinction ratio E(182nm-V)/E(B-V) --- E1800 Extinction ratio E(180nm-V)/E(B-V) --- E1780 Extinction ratio E(178nm-V)/E(B-V) --- E1760 Extinction ratio E(176nm-V)/E(B-V) --- E1740 Extinction ratio E(174nm-V)/E(B-V) --- E1720 Extinction ratio E(172nm-V)/E(B-V) --- E1700 Extinction ratio E(170nm-V)/E(B-V) --- E1680 Extinction ratio E(168nm-V)/E(B-V) --- E1660 Extinction ratio E(166nm-V)/E(B-V) --- E1640 Extinction ratio E(164nm-V)/E(B-V) --- E1620 Extinction ratio E(162nm-V)/E(B-V) --- E1600 Extinction ratio E(160nm-V)/E(B-V) --- E1580 Extinction ratio E(158nm-V)/E(B-V) --- E1560 Extinction ratio E(156nm-V)/E(B-V) --- E1540 Extinction ratio E(154nm-V)/E(B-V) --- E1520 Extinction ratio E(152nm-V)/E(B-V) --- E1500 Extinction ratio E(150nm-V)/E(B-V) --- E1480 Extinction ratio E(148nm-V)/E(B-V) --- E1460 Extinction ratio E(146nm-V)/E(B-V) --- E1440 Extinction ratio E(144nm-V)/E(B-V) --- E1420 Extinction ratio E(142nm-V)/E(B-V) --- E1400 Extinction ratio E(140nm-V)/E(B-V) --- E1380 Extinction ratio E(138nm-V)/E(B-V) --- E1360 Extinction ratio E(136nm-V)/E(B-V) --- E1340 Extinction ratio E(134nm-V)/E(B-V) --- E1320 Extinction ratio E(132nm-V)/E(B-V) --- E1300 Extinction ratio E(130nm-V)/E(B-V) --- E1280 Extinction ratio E(128nm-V)/E(B-V) --- E1260 Extinction ratio E(126nm-V)/E(B-V) --- Francois Ochsenbein CDS 1998 Apr 22 UNKNOWN UNKNOWN The data on tape were kindly supplied to CDS by P. Patriarchi (Osservatorio di Arcetri, Firenze, Italy) in 1987. The original data set contained 2 files, a description, and a set of 23 tables of 92 records each, each table providing the extinctions E(lambda-V)/E(B-V) for five stars. These tables were transformed in the large atlas.dat table; the positions were then added from the SIMBAD data-base. III_130.xml A Critical Catalogue of Spectroscopic Stellar Abundance Analyses 3131 III/131 Spectroscopic Stellar Abundance Analyses A Critical Catalogue of Spectroscopic Stellar Abundance Analyses J Koeppen CDS Inf. Bull. No. 34, p. 143 ??? ??? 1988 1988BICDS..34..143K III/165 : Catalogue of [Fe/H] determinations (Cayrel et al., 1992) Abundances The original catalogue (files *.ori) contains condensed descriptions of all spectroscopic abundance analyses (as far as the metallicity is derived) are given for normal stars (chemically peculiar stars are not included). Based on these descriptions, the "best" abundance determination(s) have been selected and indicated by a quality code. Index files and software tools are included in the catalog.
*The main index of analyzed stars Name Star name number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. --- SpType Spectral classification number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. --- RAh Right Ascension 1950 (hours) number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. h RAm Right Ascension 1950 (minutes) number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. min DE- Declination 1950 (sign) number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. --- DEd Declination 1950 (degrees) number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. deg DEm Declination 1950 (minutes) number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. arcmin Vmag Visual magnitude (from SIMBAD) number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. mag FeClass Iron abundance given in classes The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. --- Qual Quality of best analysis the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. number= The iron abundance is given in classes of [Fe/H] (log(Fe/H) relative to the abundance of the Sun) : + [Fe/H] >= +0.3 overabundance 0 -0.3 < [Fe/H] <= +0.3 solar abund. - -0.6 < [Fe/H] <= -0.3 under abund. -- -1.0 < [Fe/H] <= -0.6 ditto --- -2.0 < [Fe/H] <= -1.0 ditto ---- [Fe/H] <= -1.0 ditto ? Fe/H either not determined (e.g. in hot stars) or the abundances from the available analyses differ wildly from each other, e.g. in Vega and Deneb. As a consequence those studies which use such a star as a reference, also inherit this question mark! number= the codes are: R "RECOMMENDABLE" State-of-the-art analysis or nearly so: use of models to take fully into account the temperature stratification in the atmosphere, use of appropriate line-blanketing and NLTE-effects where necessary. Use of the broadest possible observational data, both in respect of wavelengths (IR...UV where appropriate), and variety (scans, photometry, line profiles). L "LIMITATIONS": Not quite the best possible analysis by today's(1987) means. The analysis is recommendable despite some limitations. Examples: == using un-blanketed models for cool stars, for which line-blanketed models are necessary and available; == using only optical data for hot stars, where the most important part of the spectrum lies in the ultraviolet; == using single slab models('coarse analysis') though model atmospheres are available -- J. Koeppen accepts only differential studies. I "IMPROVEMENT NEEDED": Analysis with serious limitations, such as == absolute curve-of-growth analysis; == very limited observational base. Therefore it could be desirable to have this star re-observed or the data re-analyzed with more modern techniques. ( ) Brackets indicate that this is the only analysis available ? Question mark indicates that information about the analysis method was found to be insufficient to make a definitive choice of the quality grade, e.g.: == paper mentions analysis only very briefly. --- Joachim Koeppen, Francois Ochsenbein Strasbourg Obs. 1997 Mar 05 III_131.xml New Galactic Carbon Stars Found on Southern, Near-Infrared Spectrum Plates 3132 III/132 Southern Galactic Carbon Stars - Near-IR Spectra New Galactic Carbon Stars Found on Southern, Near-Infrared Spectrum Plates D J MacConnell Astron. J 96 354 1988 1988AJ.....96..354M Stars, carbon Over 400 cool carbon stars were found on near-infrared spectrum plates of low-dispersion taken along the southern galactic plane. This represents an approximate 10% increase in the number of such stars known.
About 4000 optically detected carbon stars are known in the Galaxy, largely concentrated toward the galactic plane and to galactocentric distances greater than the solar circle, and significant numbers have been detected in the Magellanic Clouds and other Local Group galaxies. They are readily distinguished from stars of the normal, oxygen-rich sequence by the presence of strong bands of diatomic carbon (the defining characteristic) and of CN in their spectra, and the majority of the galactic ones have been found on red and near- infrared (lambda < 0.9 u) photographic plates taken with objective prisms mounted on Schmidt telescopes. In the early 1970's MacConnell began taking infrared plates of disper- sion 3400 A/mm at the A-band with the Curtis Schmidt telescope at Cerro Tololo to search for cool supergiants and other stars of interest. Plates were taken along the full galactic half-circle, from l=210 to l=30, covering a band roughly 13 degrees wide centered on the galactic plane. There are typically three unwidened I-N plates on each 5x5-degree field of 5 min, 30 min, and 60 min exposure; the deep plates are ammonia-sensitized and reach I~13. The spectra cover the 6800-8800 A region, and the features which distinguish carbon stars in this region are the strong CN bands at 7945, 8125, and 8320 A. In order for a star to be classified as carbon, it must show C bands, but these are present only blueward of the spectral range used. Stars with CN bands strong enough to be seen at this low dispersion are invariably carbon stars, usually of the cool N variety, but a survey of this type will find relatively few of the weaker-banded stars of the warmer R subtype. Table I presents the new carbon stars found, in order of R.A. 1950, as well as several dozen stars in Stephensons's catalogue (column 'GCCCS') for which improved coordinates were obtained in the present program. are accurate to about 5 arcsec in declination and to about 3 arcsec in right ascension. The visual magnitudes are estimated from a mean calibration applied to a set of direct, visual region plates of 5 min exposure taken with the same telescope, and the error is probably of the order of 1 mag.
The catalog id The number of the entry --- RAh Right ascension hours (1950) h RAm Right ascension minutes (1950) min RAs Right ascension seconds (1950) s u_RAs Uncertainty flag on RA --- DE- Declination sign (1950) --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin DEs Declination seconds (1950) arcsec u_DEs Uncertainty flag on Declination --- RAh0 Right ascension hours (1900) h RAm0 Right ascension minutes (1900) min RAs0 Right ascension seconds (1900) s u_RAs0 Uncertainty flag on 1900 RA --- DE-0 Declination sign (1900) --- DEd0 Declination degrees (1900) deg DEm0 Declination minutes (1900) arcmin DEs0 Declination seconds (1900) arcsec u_DEs Uncertainty flag on 1900 dec. --- gt Upper limit sign --- V Estimated V magnitude mag u_V Uncertainty flag on V --- GCCCS Number in Stephenson's catalog Stephenson, Bruce, 1973 "A General Catalogue of Cool Carbon Stars" Publ. Warner and Swasey Observ. Vol. 1, no. 4. For stars 372, 403, 415, and 425, the GCCCS number is replaced by unc. --- IRASh Right ascension part of IRAS number --- IRASm Declination part of IRAS number --- u_IRASh Indicates uncertainty in IRAS no. --- comp Component of multiple system --- Nancy Grace Roman/Gail L. Schneider ADC/SSDOO 1996 Feb 26 III_132.xml Catalogue of two-dimensional spectral types for the HD stars. Vol.4 3133 III/133 Michigan Catalogue of HD stars, Vol.4 Catalogue of two-dimensional spectral types for the HD stars. Vol.4 N Houk M Smith-Moore Ann Arbor, Dept. of Astronomy, Univ. of Michigan ??? ??? 1988 1988MSS...C04....0H MK spectral classification Spectral types Plate data This volume of the catalog contains all HD stars in the declination range -26 degrees up to and including -12 degrees (equinox 1900) and is part of a series of catalogs in the University of Michigan program of systematic reclassification in the MK system of the entire "Henry Draper Catalogue" (HD).
The Catalogue (vol.4) HD Henry Draper Catalog (HD) number --- Case if sp. type has lower case in printed ver. --- n_SpType if spectral type is from HD Catalog --- SpType Spectral type --- Ave_Flag if classification used is an average. --- q_SpType Quality of the classification, see adc.doc --- Remark Remark (see adc.doc Appendix A for description) --- Ptg Photographic magnitude from HD catalog mag Var_Flag 'V' if star is known or suspected variable --- RAh Hours RA, epoch 1900.0 h RAm Minutes RA, epoch 1900.0 min RAs Seconds RA, epoch 1900.0 s DE- Sign Dec, epoch 1900.0 --- DEd Degrees Dec, epoch 1900.0 deg DEm Minutes Dec, epoch 1900.0 arcmin DEs Seconds Dec, epoch 1900.0 arcsec precRAm Centennial precession in RA, minutes 0.01min/yr precRAs Centennial precession in RA, seconds 0.01s/yr precDE-s Centennial precession in Dec, sign 0.01arcmin/yr precDEm Centennial precession in Dec, minutes 0.01arcmin/yr precDEs Centennial precession in Dec, seconds 0.01arcsec/yr GLON Galactic longitude deg GLAT Galactic latitude deg DM Durchmusterung identification ('BD', 'CD', or 'CP' in bytes 93-94; -ZZNNNNN in bytes 95-102) --- SAO SAO Catalog number --- Plate1 Plate code #1 (see file plates.dat) --- Plate2 Plate code #2 (see file plates.dat) --- Plate3 Plate code #3 (see file plates.dat) --- Plate4 Plate code #4 (see file plates.dat) --- Notes (to vol.4) HD Henry Draper Catalog (HD) number --- Remark Remarks in free form text --- Summary of Plates Code Plate code --- Number Plate Number --- Date Exposure date --- adc.doc Documentation by Wayne H. Warren Jr. changes.txt List of errors corrected as reported by Shiro Nishimura [ADAC/NAOJ] Francois Ochsenbein CDS 1994 Dec 08 UNKNOWN UNKNOWN * 22-Nov-1993: list of plates added at CDS * 08-Dec-1994: list of plates provided by Shiro Nishimura [ADAC/NAOJ] III_133.xml Radial Velocities of Bright Southern Stars. V. 146 Population II F Stars and Related Objects 3134 III/134 Radial Velocities of Bright Population II F Stars Radial Velocities of Bright Southern Stars. V. 146 Population II F Stars and Related Objects J Andersen B Nordstroem Astron. & Astrophys. Suppl. 62 355-363 1985 1985A&AS...62..355A III/105 : Radial Velocities of Southern Stars with CORAVEL (Andersen+ 1995) Andersen, J. and Nordstrom, B. 1985, Astron. Astrophys. Suppl. Ser., 62, 355. Andersen, J. 1987, private communication. Jeffers, H. M., van den Bos, W. H., and Greeby, F. M. 1963, Publ. Lick Obs., 21. Olsen, E.H. 1983, A&AS, 55 Radial velocities Stars, A-type Stars, F-type Stars, G-type Stars, population II This catalog presents new radial velocity determinations, based on 20 A/mm coude plates, for 146 southern stars brighter than m(v) = 8.3. Drawn from the catalog of uvby-beta photometry of southern A5-G0 stars by Olsen (1983), the program stars are certain or suspected Population II stars. One triple-lined and 10 double-lined binaries have been detected, including HD 210737, for which a preliminary orbit has been derived. Notes on spectral peculiarities are given. The catalog is in two files. The first file lists HD number, heliocentric Julian date of observation, radial velocity with error and number of lines observed for both the primary and secondary stars, rotation class, and remarks for each observation. The second file contains additional remarks to the data of the first file, sorted by HD number.
Observations HD HD number --- HDsuffix HD suffix Component designation as listed in Jeffers et al. (1963) When bytes 1-6 are blank, the data in this record refer to the previous object. --- HJD Hel. Jul. date Heliocentric Julian date of the observation (-2,440,000) d weight * = half weight given to observation Weight flag. "*" indicates that the observation has been given half weight. --- RV1 Rad. vel. of the primary star km/s e_RV1 Internal mean error of the RV1 km/s Num1 Number of lines measured in determining RV1 --- RV2 Rad. vel. of the secondary star (if any) km/s e_RV2 Internal mean error of the RV2 km/s Num2 Num. lines measured in determining RV2 --- RotClass Rotation class Rotation class Single-digit integer indicating the "rotation class assigned from the measured line widths." The classes and corresponding limits in v sin i are as follows (km/s): class v sin i -- ------- 0 < 15 1 16 - 30 2 31 - 60 3 61- 100 4 101- 150 5 > 150 --- rem Remarks, binarity, variability The following abbreviations are used: C Preliminary CORAVEL results differ from the results of this catalog by 4 km/s or more. REM An additional remark concerning this object can be found in the second file. SB2 Double-lined binary (as indicated in the literature or by preliminary CORAVEL results) VAR Variability --- Remarks HD HD number --- suffix HD suffix Component designation as listed in Jeffers et al. (1963) --- rem Remark Text of the remark. When bytes 1-8 are blank this record continues the remark for the last object. --- C.-H. Joseph Lyu Hughes STX/NASA 1997 Jan 08 The original ADC documentation by A.C. Raugh (1988) was used to create this ReadMe file. UNKNOWN UNKNOWN Radial Velocities of Bright Southern Stars. V. 146 Population II F Stars and Related Stars (RVF) was kindly supplied to the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, by Dr. J. Andersen over BITNET in September 1987, in a format very similar to that described above. Observations and notes were broken into separate files, blank Lines between observations of different objects were removed from the first file, and blank columns were removed in both files. III_134.xml Henry Draper Catalogue and Extension 1 (HD,HDE) 3135A III/135A Henry Draper Catalogue and Extension Henry Draper Catalogue and Extension 1 (HD,HDE) A J Cannon E C Pickering Harv. Ann. 91-100 ??? ??? 1918-1924 1924hdhc.bookQ....C Spectral types Surveys An updated, corrected, and extended machine-readable version of The Henry Draper Catalogue (HD, Cannon & Pickering 1918-1924) is available with documentation from the Astronomical Data Center (ADC) as of April 1989. Published and unpublished errors discovered in the previous version have been corrected; letters indicating supplemental stars in the BD have been moved to a new byte to distinguish them from double-star components; and the machine-readable portion of The Henry Draper Extension (HDE) (HA 100; Cannon 1925-1936) has been converted to the same format as the main catalog with additional data added as necessary. The catalog lists HD numbers, Durchmusterung numbers, positions for equinox B1900, photovisual and photographic magnitudes, spectral types, codes for the intensity of the spectra used, and remarks.
The catalogue HD Henry Draper Catalog (HD) number number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. --- DM Durchmusterung identification number=1 the DM number is composed of: Bytes 7-8: catalog ID, 'BD', 'CD', 'CP', or 'AG' for AGK1 stars (zones +50 to +59) not in the BD Bytes 9-16: Durchmusterung catalog number, SZZNNNNN. For AG zones, the ZZ field contains the lowest declination zone in the appropriate catalog (50 or 55) Byte 17: BD supplement letter (catalogue <I/71> by Warren and Kress) Byte 18: DM component identification --- RAh Hours RA, equinox B1900, epoch 1900.0 number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. h RAdm Deci-Minutes RA, equinox B1900, epoch 1900.0 number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. 0.1min DE- Sign Dec, equinox B1900, epoch 1900.0 number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. --- DEd Degrees Dec, equinox B1900, epoch 1900.0 number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. deg DEm Minutes Dec, equinox B1900, epoch 1900.0 number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. arcmin q_Ptm Code for Ptm: 0 = measured, 1 = value inferred from Ptg and spectral type number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. --- Ptm Photovisual magnitude number=2 the following codes are used for the magnitudes: 20.0 nebula (Neb in published catalog) 30.0 variable (var. in published catalog) 40.0 nova (Nov. in published catalog) 50.0 cluster (Cl. in published catalog) blank no value in published catalog mag n_Ptm 'C' if Ptm is combined value with Ptg number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. --- q_Ptg Code for Ptg: 0 = measured, 1 = value inferred from Ptm and spectral type number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. --- Ptg Photographic magnitude number=2 the following codes are used for the magnitudes: 20.0 nebula (Neb in published catalog) 30.0 variable (var. in published catalog) 40.0 nova (Nov. in published catalog) 50.0 cluster (Cl. in published catalog) blank no value in published catalog mag n_Ptg 'C' if Ptg is combined value for this entry and the following or preceding entry number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. --- SpType Spectral type number= According to W. H. Warren Jr., 194629 is identical to 194648 and the latter should be deleted. --- Intensity Photographic intensity of spectrum number=3 this intensity is a number between 1 and 10, but has the value 14 for HD 35041, and value 'B' for HD 37788 and 41366 --- Remarks Remarks, see note number=4 D = Entry deleted (see adc.doc) E = Image at edge of plate G = Position and BD number taken directly from AGK1 and precessed to 1900 M = Multiple images used (see adc.doc) R = Remark in the published catalog * = Spectral type refers a cluster, nebula or nebulous star. (see adc.doc) --- adc.doc Documentation by Nancy G. Roman and Wayne H. Warren Jr (1985) Francois Ochsenbein CDS 1993 Oct 11 UNKNOWN UNKNOWN * February 1985: see the attached file "adc.doc" by Nancy G. Roman and Wayne H. Warren Jr. (document NSSDC/WDC-A-R&S 84-18); its section 4 described the story of the catalog. * October 1993: the following few modifications have been added at CDS (a) insertion of the decimal point for Ptm and Ptg fields (b) three stars had a declination "-6860" corrected to "-6900": 269534, 269975, 270350 (c) a 0 digit missing in the DEm field of stars 16110 16112 16126 16131 16138 16150 16156 16183 16187 16189 has been added (d) the spectrum of star 4815 has been corrected * 16-Apr-1994: Following a note by Sh. Nishimura (NAO Japan), about 60 remarks E and P (emission and peculiar) were changed to lowercase letters. BD designation of star 237694 have been changed from BD+567 1286 to BD+56 1286. * 02-Jan-1996: List of Errata by W.H. Warren Jr. <w3whw@gibbs.gsfc.nasa.gov> * 08-Nov-1996: The following errors reported by W. H. Warren were corrected: ============================================== HD Datum For Read Remarks ---------------------------------------------- 11502* DM BD+18 243 B BD+18 243 A 11503* DM BD+18 243 A BD+18 243 B 43436* DM BD+67 424 A BD+67 423a DMSup * 50227* DM BD+23 1523 A BD+23 1523 No comp. 51295* DM BD+23 1554 A BD+23 1554 No comp. 54052* DM BD+06 1526 A BD+06 1526 No comp. 135780* Dec -41 57 -41 47 MHD2 144069* DM BD-10 4237 A BD-10 4237 B 144070* DM BD-10 4237 B BD-10 4237 A 159000* DM BD+44 2722 B BD+44 2721a DMSup * 159001* DM BD+44 2722 B BD+44 2722 192788* DM BD+30 3960 A BD+30 3960a DMSup * 193877* DM BD+01 3984 BD-00 3984 194629* DM BD+74 858 A BD+74 858 AB dupes 194648* Delete (use code "D") = 194629 228312* DM --- BD+37 3826a BDSup. * 242495* DM --- BD+17 893 AG+17 472 267646* DM BD+27 1293 BD+27 1293 A 267647* DM BD+27 1294 A BD+27 1293 B 267648* DM BD+27 1294 B BD+27 1294 from WDS 268053* DM --- BD+33 1455 AG+33 725 III_135A.xml A Catalogue of Spectroscopically Identified Hot Subdwarf Stars 3137 III/137 Spectroscopically Identified Hot Subdwarf Stars A Catalogue of Spectroscopically Identified Hot Subdwarf Stars D Kilkenny U Heber J S Drilling S.Afr. Astron. Obs. Circ. 12 1-80 1988 1988SAAOC..12....1K Stars, population II The catalog contains data for 1225 spectroscopically classified hot subdwarf stars. It excludes central stars of planetary nebulae but includes stars in binary systems. The data assembled include, where available, alternative designations, accurate coordinates, UBV and uvby photometry, spectral types and determinations of effective temperature and surface gravity.
Prior to 1986 there were around 200 spectroscopically classified hot subdwarf stars. The Palomar-Green survey (Green et al., 1986) detected over 900 hot subdwarfs, mostly in the North Galactic Cap and mostly previously unknown objects; the Kitt-Peak_Downes survey found another 60 near the Galactic Plane (Downes, 1986). These form the basis of the present catalog but new subdwarfs are continually being found by spectroscopic surveys of photographically discovered faint blue star samples; examples are the work of Wegner and his co-workers on the Kiso survey (Wegner et al., 1985, 1986, 1987) and of Kilkenny and Muller (1987) on southern discoveries by Luyten and collaborators (e. g. Haro and Luyten, 1962; Luyten and Anderson, 1958, 1959, 1967). Only stars for which a spectroscopic classification exists have been included. There is a significant probability that stars with only photometric classifications can be normal high-latitude B stars, white dwarfs or cataclysmic variable, for example. Hot subdwarfs in binary systems have been included but not planetary nebulae nuclei classified 'sd' since the latter have been cataloged elsewhere. Although there is not a universally accepted classification scheme for hot subdwarfs, it is fairly clear that the main criterion is a surface gravity higher than that of hot main sequence stars but less than that of hot white dwarfs. Also, hot subdwarf stars typically show helium abundance anomalies.
Data on hot subdwarf stars ID Star identification The star name from the original discovery catalog, unless a more common name (such as an HD designation) exists. This has been done even when the discovery catalog gave a 'faint blue object' type rather than a spectroscopic classification because much of the published literature naturally uses the 'discovery' name. Some stars in the data file occupy multiple records. In this case, ID and desig are repeated for all applicable records. --- desig RA/Dec designation Where an RA/Dec designation exists, this has been included using the convention RA (hours, minutes, decimal minutes), sign, Dec (degrees, minutes) with truncation for the last figure in RA and Dec (this avoids occasional rounding ambiguities). The Kiso surveys (Noguchi et al., 1980; Kondo et al., 1984) use rounding to determine the RA/Dec type nomenclature and this has been retained in this catalog to avoid confusing the identifi- cation in published material. Thus, there are sometimes small differences between the KUV and PG names; in this case, both are given. --- RAh Right Ascension (1950) hours h RAm Right Ascension (1950) minutes min n_RAm Right Ascension (1950) sec. or decimal min. Coordinates for 1950 quoted to second and arcsecond accuracy where possible. More accurate co-ordinates can sometimes be found in the source catalogues. If byte 28 is blank, then value in this field is Right Ascension seconds. If byte 28 contains a decimal point, then this field is a continuation of RAm. --- DE- Declination (1950) sign --- DEd Declination (1950) degrees deg DEm Declination (1950) arcminutes arcmin n_DEm Declination (1950) arcsec or decimal arcmin If byte 38 is blank, then value in this field is Declination seconds. If byte 38 contains a decimal point, then this field is a continuation of DEm. --- Name Alternative name for star Alternative names. The authors have tried to include as many common names as possible for each object but have not exhaustively cross-indexed all possible catalogs. Durchmusterung designations for HD stars are not included although such will almost always exist. --- V V magnitude The Johnson or Stroemgren photometry. Because these data occupy the same columns, the immediate way to tell which is which is that the UBV photometry has three quantities; the uvby has four. Hence, where partial information is available in the literature (E.g. V and (B-V) or V, (b-y) and m1) only the magnitude has been listed in this catalog and the original reference must be consulted for the data. Occasionally, a reference will contain other photometric information such as RI or even infrared photometry, so it is always worth checking the original source. mag u_V Uncertainty flag on V --- color1 (B-V) or (b-y) mag u_color1 Uncertainty flag on color1 --- color2 (U-B) or m1 mag u_color2 Uncertainty flag on color2 --- color3 c1 or blank mag r_V A reference for the photometry --- Sp Spectral type Spectral type quoted directly from the literature. No attempt has been made to put the classifications on a uniform system. Probably this should be left until a clear picture of the evolution of hot subdwarf stars emerges. Originally the classes 'sd B' and 'sd O' were recognized by broad Balmer line absorption and the early confluence of the Balmer series; B types were classified by weak or non-existent helium lines and O types by the presence of HeII 4686 or other HeII lines (see e. g. Sargent and Searle 1968). Liebert (1987) accept the sd B, OB, O sequence as one of increasing temperature and helium abundance but propose a new 'hot sd' category with Teff > 60000 K which overlaps with planetary nebula nuclei, PG 1159 stars and hot white dwarfs. Recent spectroscopic analyses (Heber and Hunger 1987, Mendez et al. 1988) indicate that there is indeed an overlap of hot sdO stars with central stars of planetary nebulae and vice versa. In the Palomar-Green survey, Green et al. (1986) use a scheme which is worth summarizing here because the PG-classified stars are a substantial fraction of our catalogue. Briefly: sd B = broad Balmer series absorption sd B-O = sd B stars with very weak HeI 4471 sd OA = strong Balmer absorption with HeI 4471 and often HeI 4026 sd OB = dominated by HeI and HeII lines; often Balmer absorption present sd OC = dominated by HeII absorption; possibly weak HeI 4471 and Balmer series blended with HeII Brackett lines sd OD = 'pure' HeI absorption; weak or absent H and HeII sd O = HeII 4686 and often HeI 4471 present but signal/noise too poor for further classification sd = broad Balmer series absorption but signal/noise too poor for further classification However, the PG classification 'sdOB' is a helium-rich sdO star quite different from the Baschek and Norris (1975) helium-weak 'sdOB'. To separate the authors have introduced the nomenclature sdO(A), sdO(B), sdO(C) and sdO(D) to replace the PG sdOA, ...... , sdOD subtypes. --- r_Sp A reference for the spectral type --- l_Teff Limit flag on Teff --- Teff Log of effective temperature log (effective temperature). Often this is published as K temperature; we have given the logarithm to two decimal places only --- u_Teff Uncertainty flag on Teff --- l_log(g) Limit flag on log(g) --- log(g) Log of surface gravity --- u_log(g) Uncertainty flag on log(g) --- r_Teff Reference for Teff and log(g) --- References ref Reference code Code as it appears in r_* fields of data.dat --- text Text of reference --- Julie Anne Watko ADC/SSDOO 1996 May 22 The catalogue was sent to the ADC by Dr. Kilkenny for which we thank him. This document is nearly a verbatim copy of the published text with the exception of the format tables by Julie Anne Watko, and minor changes, particularly the elimination of the first-person references. III_137.xml A Compendium of Equivalent Width Measures 3139A III/139A Equivalent Width Measures A Compendium of Equivalent Width Measures R E Luck Case Western Reserve Univ. ??? ??? 1990 1990 Equivalent widths The files in this data set contain equivalent width measures made in the course of a number of published studies for four types of objects: mid-to-late supergiants, metal-deficient red giants, subgiant CH stars, and G/K giants. The files include identified atomic and ionic species, wavelength, lower excitation potentials and log(gf) values. It includes also a Fortran program file to read the data. Subgiant CH stars in the data are late F to early G stars whose spectra exhibit strong CH, Sr II, and sometimes Ba II features.
Supergiant 1 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star 1: Alpha Aqr 10-4nm n_EW1 analysis flag Character flag indicating whether or not the line was retained in the analysis. "-" : no information "*" : line used in analysis " " : line not used in analysis --- EW2 equivalent width for star 2: Beta Aqr 10-4nm n_EW2 analysis flag --- EW3 equivalent width for star 3: Beta Dra 10-4nm n_EW3 analysis flag --- EW4 equivalent width for star 4: 145 CMa 10-4nm n_EW4 analysis flag --- EW5 equivalent width for star 5: 31 Cyg 10-4nm n_EW5 analysis flag --- EW6 equivalent width for star 6: Epsilon Gem 10-4nm n_EW6 analysis flag --- EW7 equivalent width for star 7: Epsilon Peg 10-4nm n_EW7 analysis flag --- EW8 equivalent width for star 8: Eta Per 10-4nm n_EW8 analysis flag --- EW9 equivalent width for star 9: HR 8726 10-4nm n_EW9 analysis flag --- EW10 equivalent width for star 10: Mu Per 10-4nm n_EW10 analysis flag --- EW11 equivalent width for star 11: Omi 1 CMa 10-4nm n_EW11 analysis flag --- EW12 equivalent width for star 12: Psi And 10-4nm n_EW12 analysis flag --- EW13 equivalent width for star 13: 56 Peg 10-4nm n_EW13 analysis flag --- EW14 equivalent width for star 14: 9 Peg 10-4nm n_EW14 analysis flag --- EW15 equivalent width for star 15: 1 Pup 10-4nm n_EW15 analysis flag --- EW16 equivalent width for star 16: Xi Cyg 10-4nm n_EW16 analysis flag --- EW17 equivalent width for star 17: Xi Pup 10-4nm n_EW17 analysis flag --- EW18 equivalent width for star 18: Zeta Aur 10-4nm n_EW18 analysis flag --- EW19 equivalent width for star 19: Zeta Cep 10-4nm n_EW19 analysis flag --- Supergiant 2 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: 104 Aqr 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: BU Gem (1) ; 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: BU Gem (2) ; 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: 3 Cet 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: 25 Gem 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: 41 Gem 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: HD 16901 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: HD 187238 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: HD 187299 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: HD 33299 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: HD 35601 10-4nm n_EW11 -=no info; *=line used; " "=not used --- EW12 equivalent width for star: HD 37387 10-4nm n_EW12 -=no info; *=line used; " "=not used --- EW13 equivalent width for star: HD 38247 10-4nm n_EW13 -=no info; *=line used; " "=not used --- EW14 equivalent width for star: HD 39949 10-4nm n_EW14 -=no info; *=line used; " "=not used --- EW15 equivalent width for star: HD 42454 10-4nm n_EW15 -=no info; *=line used; " "=not used --- EW16 equivalent width for star: HD 44391 10-4nm n_EW16 -=no info; *=line used; " "=not used --- EW17 equivalent width for star: HD 45829 10-4nm n_EW17 -=no info; *=line used; " "=not used --- EW18 equivalent width for star: HD 48640 10-4nm n_EW18 -=no info; *=line used; " "=not used --- EW19 equivalent width for star: HD 49068 10-4nm n_EW19 -=no info; *=line used; " "=not used --- EW20 equivalent width for star: HD 63302 10-4nm n_EW20 -=no info; *=line used; " "=not used --- EW21 equivalent width for star: HR 3459 10-4nm n_EW21 -=no info; *=line used; " "=not used --- EW22 equivalent width for star: NO Aur 10-4nm n_EW22 -=no info; *=line used; " "=not used --- EW23 equivalent width for star: 12 Peg 10-4nm n_EW23 -=no info; *=line used; " "=not used --- EW24 equivalent width for star: 119 Tau 10-4nm n_EW24 -=no info; *=line used; " "=not used --- EW25 equivalent width for star: Theta Del 10-4nm n_EW25 -=no info; *=line used; " "=not used --- EW26 equivalent width for star: TV Gem 10-4nm n_EW26 -=no info; *=line used; " "=not used --- EW27 equivalent width for star: WY Gem 10-4nm n_EW27 -=no info; *=line used; " "=not used --- Supergiant 3 Ionb Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: HD 10494 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: HD 11092 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: HD 11544 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: HD 14622 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: HD 163428 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: HD 16901 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: HD 172365 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: HD 174104 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: HD 174947 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: HD 17958 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: HD 180028 10-4nm n_EW11 -=no info; *=line used; " "=not used --- EW12 equivalent width for star: HD 18391 10-4nm n_EW12 -=no info; *=line used; " "=not used --- EW13 equivalent width for star: HD 185622 10-4nm n_EW13 -=no info; *=line used; " "=not used --- EW14 equivalent width for star: HD 190323 10-4nm n_EW14 -=no info; *=line used; " "=not used --- EW15 equivalent width for star: HD 202380 10-4nm n_EW15 -=no info; *=line used; " "=not used --- EW16 equivalent width for star: HD 207119 10-4nm n_EW16 -=no info; *=line used; " "=not used --- EW17 equivalent width for star: HD 207489 10-4nm n_EW17 -=no info; *=line used; " "=not used --- EW18 equivalent width for star: HD 207991 10-4nm n_EW18 -=no info; *=line used; " "=not used --- EW19 equivalent width for star: HD 208606 10-4nm n_EW19 -=no info; *=line used; " "=not used --- EW20 equivalent width for star: HD 219978 10-4nm n_EW20 -=no info; *=line used; " "=not used --- EW21 equivalent width for star: HD 224165 10-4nm n_EW21 -=no info; *=line used; " "=not used --- EW22 equivalent width for star: HD 4362 10-4nm n_EW22 -=no info; *=line used; " "=not used --- EW23 equivalent width for star: HD 4817 10-4nm n_EW23 -=no info; *=line used; " "=not used --- EW24 equivalent width for star: HD 611 10-4nm n_EW24 -=no info; *=line used; " "=not used --- EW25 equivalent width for star: HD 9973 10-4nm n_EW25 -=no info; *=line used; " "=not used --- EW26 equivalent width for star: Nu 1 Sgr 10-4nm n_EW26 -=no info; *=line used; " "=not used --- EW27 equivalent width for star: VV Cep 10-4nm n_EW27 -=no info; *=line used; " "=not used --- Supergiant 4 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: HR 4614 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: HD 124602 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: HD 154679 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: HD 163578 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: +2 1406 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: R Pup 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: CD -57 3502 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: -45 10988 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: -35 11532 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: V500 Sco(B) 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: HD 166263 10-4nm n_EW11 -=no info; *=line used; " "=not used --- EW12 equivalent width for star: HD 51935 10-4nm n_EW12 -=no info; *=line used; " "=not used --- EW13 equivalent width for star: -21 1990 10-4nm n_EW13 -=no info; *=line used; " "=not used --- EW14 equivalent width for star: -60 3636 10-4nm n_EW14 -=no info; *=line used; " "=not used --- EW15 equivalent width for star: -60 3621 10-4nm n_EW15 -=no info; *=line used; " "=not used --- EW16 equivalent width for star: HD 138110 10-4nm n_EW16 -=no info; *=line used; " "=not used --- EW17 equivalent width for star: HD 53007 10-4nm n_EW17 -=no info; *=line used; " "=not used --- EW18 equivalent width for star: HD 58790 10-4nm n_EW18 -=no info; *=line used; " "=not used --- EW19 equivalent width for star: HD 63302 10-4nm n_EW19 -=no info; *=line used; " "=not used --- EW20 equivalent width for star: -29 13788 10-4nm n_EW20 -=no info; *=line used; " "=not used --- EW21 equivalent width for star: V500 Sco(C) 10-4nm n_EW21 -=no info; *=line used; " "=not used --- EW22 equivalent width for star: HD 167175 10-4nm n_EW22 -=no info; *=line used; " "=not used --- EW23 equivalent width for star: HD 167884 10-4nm n_EW23 -=no info; *=line used; " "=not used --- EW24 equivalent width for star: HD 166058 10-4nm n_EW24 -=no info; *=line used; " "=not used --- EW25 equivalent width for star: HD 151834 10-4nm n_EW25 -=no info; *=line used; " "=not used --- EW26 equivalent width for star: -30 14738 10-4nm n_EW26 -=no info; *=line used; " "=not used --- EW27 equivalent width for star: HD 165553 10-4nm n_EW27 -=no info; *=line used; " "=not used --- EW28 equivalent width for star: AX Sgr 10-4nm n_EW28 -=no info; *=line used; " "=not used --- EW29 equivalent width for star: +59 594 10-4nm n_EW29 -=no info; *=line used; " "=not used --- EW30 equivalent width for star: +54 651 10-4nm n_EW30 -=no info; *=line used; " "=not used --- EW31 equivalent width for star: +4 1370 10-4nm n_EW31 -=no info; *=line used; " "=not used --- EW32 equivalent width for star: HD 49102 10-4nm n_EW32 -=no info; *=line used; " "=not used --- EW33 equivalent width for star: HD 52801 10-4nm n_EW33 -=no info; *=line used; " "=not used --- EW34 equivalent width for star: HD 55810 10-4nm n_EW34 -=no info; *=line used; " "=not used --- EW35 equivalent width for star: HD 6474 10-4nm n_EW35 -=no info; *=line used; " "=not used --- EW36 equivalent width for star: +55 780 10-4nm n_EW36 -=no info; *=line used; " "=not used --- EW37 equivalent width for star: HD 61730 10-4nm n_EW37 -=no info; *=line used; " "=not used --- EW38 equivalent width for star: HD 62236 10-4nm n_EW38 -=no info; *=line used; " "=not used --- EW39 equivalent width for star: HD 53177 10-4nm n_EW39 -=no info; *=line used; " "=not used --- EW40 equivalent width for star: HD 164472 10-4nm n_EW40 -=no info; *=line used; " "=not used --- EW41 equivalent width for star: HD 151097 10-4nm n_EW41 -=no info; *=line used; " "=not used --- EW42 equivalent width for star: HD 152254 10-4nm n_EW42 -=no info; *=line used; " "=not used --- EW43 equivalent width for star: CPD -41 11336 10-4nm n_EW43 -=no info; *=line used; " "=not used --- EW44 equivalent width for star: HD 155603 10-4nm n_EW44 -=no info; *=line used; " "=not used --- EW45 equivalent width for star: HD 160706 10-4nm n_EW45 -=no info; *=line used; " "=not used --- EW46 equivalent width for star: HD 161388 10-4nm n_EW46 -=no info; *=line used; " "=not used --- EW47 equivalent width for star: V500 Sco(A) 10-4nm n_EW47 -=no info; *=line used; " "=not used --- EW48 equivalent width for star: HD 167746 10-4nm n_EW48 -=no info; *=line used; " "=not used --- EW49 equivalent width for star: HD 167976 10-4nm n_EW49 -=no info; *=line used; " "=not used --- EW50 equivalent width for star: HD 173838 10-4nm n_EW50 -=no info; *=line used; " "=not used --- Supergiant 5 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: 14 Per 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: 41 Gem 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: BD +14 2881 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: BD +29 1061 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: BD +61 2575 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: Epsilon Gem 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: HD 12014 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: HD 162740 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: HD 173297 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: HD 17971 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: HD 179784 10-4nm n_EW11 -=no info; *=line used; " "=not used --- EW12 equivalent width for star: HD 34248 10-4nm n_EW12 -=no info; *=line used; " "=not used --- EW13 equivalent width for star: HD 34589 10-4nm n_EW13 -=no info; *=line used; " "=not used --- EW14 equivalent width for star: HD 34669 10-4nm n_EW14 -=no info; *=line used; " "=not used --- EW15 equivalent width for star: HD 36931 10-4nm n_EW15 -=no info; *=line used; " "=not used --- EW16 equivalent width for star: HD 37073 10-4nm n_EW16 -=no info; *=line used; " "=not used --- EW17 equivalent width for star: HD 40113 10-4nm n_EW17 -=no info; *=line used; " "=not used --- EW18 equivalent width for star: HD 63302 10-4nm n_EW18 -=no info; *=line used; " "=not used --- EW19 equivalent width for star: ¡HD 6474 10-4nm n_EW19 -=no info; *=line used; " "=not used --- EW20 equivalent width for star: HD 8992 10-4nm n_EW20 -=no info; *=line used; " "=not used --- EW21 equivalent width for star: W Gem 10-4nm n_EW21 -=no info; *=line used; " "=not used --- EW22 equivalent width for star: Zeta Cep 10-4nm n_EW22 -=no info; *=line used; " "=not used --- Supergiant 6 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: V378 Cen (A) 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: Kappa Pav (3); 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: Kappa Pav(4); 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: RU Cen 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: Kappa Pav (5) ; 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: CO Aur 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: U Mon 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: AI CMi 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: Kappa Pav(1); 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: Kappa Pav(2); 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: V378 Cen (B) 10-4nm n_EW11 -=no info; *=line used; " "=not used --- Supergiant 7 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: SU Cas 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: Delta Cep12/78 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: Delta Cep 8/79 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: DT Cyg 9/79 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: Eta Aql 6/78 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: Eta Aql 7/79 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: RT Aur 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: SV Vul 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: T Mon 3/78 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: T Mon 2/79 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: T Mon 4/80 10-4nm n_EW11 -=no info; *=line used; " "=not used --- EW12 equivalent width for star: TU Cas 10-4nm n_EW12 -=no info; *=line used; " "=not used --- EW13 equivalent width for star: T Vul 10-4nm n_EW13 -=no info; *=line used; " "=not used --- EW14 equivalent width for star: W Sgr 8/79 10-4nm n_EW14 -=no info; *=line used; " "=not used --- EW15 equivalent width for star: W Sgr 6/82 10-4nm n_EW15 -=no info; *=line used; " "=not used --- EW16 equivalent width for star: X Cyg 9/79 10-4nm n_EW16 -=no info; *=line used; " "=not used --- EW17 equivalent width for star: X Sgr 6/78 10-4nm n_EW17 -=no info; *=line used; " "=not used --- EW18 equivalent width for star: X Srg 7/79 10-4nm n_EW18 -=no info; *=line used; " "=not used --- EW19 equivalent width for star: RS Pup 10-4nm n_EW19 -=no info; *=line used; " "=not used --- EW20 equivalent width for star: Zeta Gem 4/78 10-4nm n_EW20 -=no info; *=line used; " "=not used --- EW21 equivalent width for star: Zeta Gem 12/78 10-4nm n_EW21 -=no info; *=line used; " "=not used --- EW22 equivalent width for star: Zeta Gem 4/80 10-4nm n_EW22 -=no info; *=line used; " "=not used --- EW23 equivalent width for star: Beta Dor 5 Jan 10-4nm n_EW23 -=no info; *=line used; " "=not used --- EW24 equivalent width for star: Beta Dor 10 Jan 10-4nm n_EW24 -=no info; *=line used; " "=not used --- EW25 equivalent width for star: Eta Aql 1982 10-4nm n_EW25 -=no info; *=line used; " "=not used --- EW26 equivalent width for star: L Car 10-4nm n_EW26 -=no info; *=line used; " "=not used --- Supergiant 8 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: Alpha Lep 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: Alpha Per 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: Iota Car 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: Canopus 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: Beta Dra 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: Delta CMa 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: Gamma Cyg 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: 32 Cyg 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: HR 2881 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: HR 4180 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: Xi Pup 10-4nm n_EW11 -=no info; *=line used; " "=not used --- Supergiant 9 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: 89 Her 29/04/83 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: 89 Her 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: 89 Her 22/06/83 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: 89 Her 23/10/88 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star:HD161796A 22/06/83 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: HD161796B 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: HR6144 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: HR7671 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: HR7671 29/06/86 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: HR7671 9/08/85 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: HR7671 11/08/85 10-4nm n_EW11 -=no info; *=line used; " "=not used --- EW12 equivalent width for star: HR7671 13/08/85 10-4nm n_EW12 -=no info; *=line used; " "=not used --- Metal Def 1 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: BD +17 3248 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: HD 110184 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: HD 184266 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: HD 204543 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: HD 216143 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: HD 218857 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: HD 2796 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: HD 4306 (A) 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: HD 4306 (B) 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: HD 6268 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: HD 122563 10-4nm n_EW11 -=no info; *=line used; " "=not used --- Metal Def 2 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: HD 2796 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: HD 4306 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: CD -30 298 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: HD 6268 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: BD -18 271 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: HD 13979 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: CD -24 1782 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: HD 26297 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: BD +6 648 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: HD 29574 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: HD 37828 10-4nm n_EW11 -=no info; *=line used; " "=not used --- EW12 equivalent width for star: HD 73394 10-4nm n_EW12 -=no info; *=line used; " "=not used --- EW13 equivalent width for star: HD 74462 10-4nm n_EW13 -=no info; *=line used; " "=not used --- EW14 equivalent width for star: HD 81192 10-4nm n_EW14 -=no info; *=line used; " "=not used --- EW15 equivalent width for star: BD +58 1218 10-4nm n_EW15 -=no info; *=line used; " "=not used --- EW16 equivalent width for star: HD 85773 10-4nm n_EW16 -=no info; *=line used; " "=not used --- EW17 equivalent width for star: HD 88609 10-4nm n_EW17 -=no info; *=line used; " "=not used --- EW18 equivalent width for star: BD +30 2034 10-4nm n_EW18 -=no info; *=line used; " "=not used --- EW19 equivalent width for star: HD 93487 10-4nm n_EW19 -=no info; *=line used; " "=not used --- EW20 equivalent width for star: TY Vir 10-4nm n_EW20 -=no info; *=line used; " "=not used --- EW21 equivalent width for star: TY Vir 10-4nm n_EW21 -=no info; *=line used; " "=not used --- EW22 equivalent width for star: BD -1 2582 10-4nm n_EW22 -=no info; *=line used; " "=not used --- EW23 equivalent width for star: HD 104893 10-4nm n_EW23 -=no info; *=line used; " "=not used --- EW24 equivalent width for star: HD 107752 10-4nm n_EW24 -=no info; *=line used; " "=not used --- EW25 equivalent width for star: HD 108317 10-4nm n_EW25 -=no info; *=line used; " "=not used --- EW26 equivalent width for star: BD +4 2621 10-4nm n_EW26 -=no info; *=line used; " "=not used --- EW27 equivalent width for star: HD 110184 10-4nm n_EW27 -=no info; *=line used; " "=not used --- EW28 equivalent width for star: HD 122563 10-4nm n_EW28 -=no info; *=line used; " "=not used --- EW29 equivalent width for star: BD +1 2916 10-4nm n_EW29 -=no info; *=line used; " "=not used --- EW30 equivalent width for star: HD 126587 10-4nm n_EW30 -=no info; *=line used; " "=not used --- EW31 equivalent width for star: BD +30 3611 10-4nm n_EW31 -=no info; *=line used; " "=not used --- EW32 equivalent width for star: HD 135148 10-4nm n_EW32 -=no info; *=line used; " "=not used --- EW33 equivalent width for star: BD +9 3063 10-4nm n_EW33 -=no info; *=line used; " "=not used --- EW34 equivalent width for star: HD 166161 10-4nm n_EW34 -=no info; *=line used; " "=not used --- EW35 equivalent width for star: HD 184711 10-4nm n_EW35 -=no info; *=line used; " "=not used --- EW36 equivalent width for star: BD -18 5550 10-4nm n_EW36 -=no info; *=line used; " "=not used --- EW37 equivalent width for star: HD 218502 10-4nm n_EW37 -=no info; *=line used; " "=not used --- CH Star 1 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: HD 11377 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: HD 182274 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: HD 204613 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: HD 216219 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: HD 4395 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: HD 88446 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: HD 89948 10-4nm n_EW7 -=no info; *=line used; " "=not used --- CH Star 2 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: HD 182274 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: HD 216219 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: HD 4395 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: HD 88446 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: HD 89948 10-4nm n_EW5 -=no info; *=line used; " "=not used --- GK Star 1 Ion Identification of atomic/ionic species --- Wavelen Wavelength of line 0.1nm low-EP lower excitation potential eV log(GF) log(statistical weight x oscillator strength) --- EW1 equivalent width for star: HR 237 10-4nm n_EW1 -=no info; *=line used; " "=not used --- EW2 equivalent width for star: HD 6833 10-4nm n_EW2 -=no info; *=line used; " "=not used --- EW3 equivalent width for star: HR 649 10-4nm n_EW3 -=no info; *=line used; " "=not used --- EW4 equivalent width for star: HR 1784 10-4nm n_EW4 -=no info; *=line used; " "=not used --- EW5 equivalent width for star: HR 1907 10-4nm n_EW5 -=no info; *=line used; " "=not used --- EW6 equivalent width for star: HR 3403 10-4nm n_EW6 -=no info; *=line used; " "=not used --- EW7 equivalent width for star: HR 3484 10-4nm n_EW7 -=no info; *=line used; " "=not used --- EW8 equivalent width for star: HR 3733 10-4nm n_EW8 -=no info; *=line used; " "=not used --- EW9 equivalent width for star: HR 4146 10-4nm n_EW9 -=no info; *=line used; " "=not used --- EW10 equivalent width for star: HR 4608 10-4nm n_EW10 -=no info; *=line used; " "=not used --- EW11 equivalent width for star: HR 4783 10-4nm n_EW11 -=no info; *=line used; " "=not used --- EW12 equivalent width for star: HR 5287 10-4nm n_EW12 -=no info; *=line used; " "=not used --- EW13 equivalent width for star: HR 5681 10-4nm n_EW13 -=no info; *=line used; " "=not used --- EW14 equivalent width for star: HR 6075 10-4nm n_EW14 -=no info; *=line used; " "=not used --- EW15 equivalent width for star: HR 6152 10-4nm n_EW15 -=no info; *=line used; " "=not used --- EW16 equivalent width for star: HR 6220 10-4nm n_EW16 -=no info; *=line used; " "=not used --- EW17 equivalent width for star: HR 6698 10-4nm n_EW17 -=no info; *=line used; " "=not used --- EW18 equivalent width for star: HR 6766 10-4nm n_EW18 -=no info; *=line used; " "=not used --- EW19 equivalent width for star: HR 6791 10-4nm n_EW19 -=no info; *=line used; " "=not used --- EW20 equivalent width for star: HR 7063 10-4nm n_EW20 -=no info; *=line used; " "=not used --- EW21 equivalent width for star: HR 7125 10-4nm n_EW21 -=no info; *=line used; " "=not used --- EW22 equivalent width for star: HR 7218 10-4nm n_EW22 -=no info; *=line used; " "=not used --- EW23 equivalent width for star: HR 7468 10-4nm n_EW23 -=no info; *=line used; " "=not used --- EW24 equivalent width for star: HR 7582 10-4nm n_EW24 -=no info; *=line used; " "=not used --- EW25 equivalent width for star: HR 7744 10-4nm n_EW25 -=no info; *=line used; " "=not used --- EW26 equivalent width for star: HR 7995 10-4nm n_EW26 -=no info; *=line used; " "=not used --- EW27 equivalent width for star: HR 8035 10-4nm n_EW27 -=no info; *=line used; " "=not used --- EW28 equivalent width for star: HR 8252 10-4nm n_EW28 -=no info; *=line used; " "=not used --- EW29 equivalent width for star: HR 8626 10-4nm n_EW29 -=no info; *=line used; " "=not used --- EW30 equivalent width for star: HR 8852 10-4nm n_EW30 -=no info; *=line used; " "=not used --- C.-H. Joseph Lyu & Paul Kuin Hughes STX/NASA 1997 Feb 25 The original description file by R. E. Luck (1990) was used to create this ReadMe file. UNKNOWN UNKNOWN Forbidden lines, surrounded by square brackets in the original data, have been changed so that the data can be represented in both ASCII and EBCDIC (some conversion tables are not consistent for brackets). The brackets are now represented by parentheses () to indicate forbidden lines. Change made at the Astronomical Data Center, NASA/GSFC, February 10, 1990. Wayne H. Warren Jr. The headers were removed from the data files so that the data could be described by a Byte-by-byte Description Feb 1997. III_139A.xml Cool Carbon stars found with the Baldone Schmidt Telescope - Version 1987 3140 III/140 Carbon stars from Baldone telescope Cool Carbon stars found with the Baldone Schmidt Telescope - Version 1987 Z Alksne A Alksnis V Ozolina I Platais Radioastrophys. Observatory Latvian Academy of Sciences, Riga ??? ??? 1987 1987 Stars, carbon This catalogue contains data on 318 cool carbon stars discovered on objective prism photographs taken with the Schmidt Telescope (80/120/240 cm) of the Radioastrophysical Observatory at Baldone near Riga. Green-yellow survey (BC Nos 1-217) is made on the ortochromatic astronomical films A-600. Reciprocial dispersion of the spectra: 600 A/mm or 1130 A/mm at H-gamma. The region of the sky covered by the survey: 1) 4.5 degrees wide zones centered on the galactic latitudes +7 and -7 degrees between longitudes 68 and 200 degrees, 2) equatorial zone at longitudes 84-96 degrees and 172-180 degrees, 3) several other separate fields with five degrees diameter. Infrared survey (BC Nos 218-318) made on the infrared Kodak plates 1N with the filter Schott RG1. Reciprocial dispersion: 2500 A/mm at the atmospheric A-band. The region of the sky covered: 1) 4.5 degrees wide zone centered on the galactic latitude +7 degrees between longitudes 128 and 140 degrees, 2) region between latitudes +9.5 and -9.5 degrees and longitudes between 80 and 96 degrees.
The Baldone Survey of Cool Carbon Stars BC The number of the star in the Survey --- RAh Right Ascension 1950 (hours) number=1 position as measured on direct red plates taken with the Schmidt Telescope and reduced using the AGK3 catalogue. h RAm Right Ascension 1950 (minutes) number=1 position as measured on direct red plates taken with the Schmidt Telescope and reduced using the AGK3 catalogue. min RAs Right Ascension 1950 (seconds) number=1 position as measured on direct red plates taken with the Schmidt Telescope and reduced using the AGK3 catalogue. s DE- Declination 1950 (sign) number=1 position as measured on direct red plates taken with the Schmidt Telescope and reduced using the AGK3 catalogue. --- DEd Declination 1950 (degrees) number=1 position as measured on direct red plates taken with the Schmidt Telescope and reduced using the AGK3 catalogue. deg DEm Declination 1950 (minutes) number=1 position as measured on direct red plates taken with the Schmidt Telescope and reduced using the AGK3 catalogue. arcmin DEs Declination 1950 (seconds) number=1 position as measured on direct red plates taken with the Schmidt Telescope and reduced using the AGK3 catalogue. arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Chart Reference for identification charts (see References below) --- SpType Spectral type: R or N or R-N number=2 the spectral classification (late R or early N) depends on density distribution of obtained spectra, thus the faint Carbon stars are denoted by C. --- l_Rmag Upper brightness limit number=3 the symbol "(" indicates an upper limit of brightness in the case of extremely faint stars. --- Rmag Photographic red magnitude number=4 photographic red magnitude, effective wavelength 0.63 microns. mag --- Indicates a range for variables --- Rmag2 Upper limit for a range number=4 photographic red magnitude, effective wavelength 0.63 microns. mag Vmag Photographic V magnitude mag --- Indicates a range for variables --- Vmag2 Upper limit for a range mag l_Bmag Upper brightness limit number=3 the symbol "(" indicates an upper limit of brightness in the case of extremely faint stars. --- Bmag Photographic B magnitude mag --- Indicates a range for variables --- l_Bmag2 Upper brightness limit number=3 the symbol "(" indicates an upper limit of brightness in the case of extremely faint stars. --- Bmag2 Upper limit for a range mag Name Designation of the variable star or its preliminary name (SVS- Soviet Variable Star) --- Ref Reference for the photometric data (see References below) --- CrossId Cross-identification number=5 Cross-identification between this catalogue and the others. The number of the star is given in cols. 103-106, and the appropriate reference, coded according to the References below, in cols. 108-109. --- Francois Ochsenbein CDS 1997 Apr 25 III_140.xml New Subdwarfs. V. Radial Velocities for 889 High-Proper-Motion Stars Measured with the Mount Wilson 100-inch Reflector 3144 III/144 Radial Velocities for High Proper Motion Stars New Subdwarfs. V. Radial Velocities for 889 High-Proper-Motion Stars Measured with the Mount Wilson 100-inch Reflector G Fouts A Sandage Astron. J. 91 1189 1986 1986AJ.....91.1189F Radial velocities Stars, subdwarf The machine-readable version of Radial Velocities of High-Proper-Motion Stars contains UBV photometry, proper motions, and radial (line-of-sight) velocities for 878 high-proper-motion stars that were selected from the subdwarf candidate list of Sandage and Fouts (1986).
The title and source document refer to data for 889 high-proper-motion stars taken from the list of subdwarf candidates compiled by Sandage and Kowal (1986). However, eleven stars found to have variable velocities are omitted from both the published table and the machine-readable file. The primary data are new radial velocities determined from 2265 measurements made from observations with the Mount Wilson 2.5-meter telescope coude spectrograph with a Reticon detector. The internal error of a single measurement was determined to be 1 sigma. = 4.7 km/s, while 88 stars in common with previously known subdwarfs gave an external error of 1 sigma. = 6.9 km/s per measure. The velocity system was determined to be on the system of the Wilson General Catalogue of Stellar Radial Velocities (Wilson 1953) to better than 1 km/s. There are 38 stars in the catalog having line-of-sight velocities larger than v(r) = 200 km/s, of which 22 are new. The source reference should be consulted for additional information concerning sample selection, instrumentation and spectral coverage, reduction procedures, and results of the data analysis.
The catalog ordered by B1950.0 right ascension flag Flag An asterisk (*) flag to indicate stars for which prior radial-velocity data were reported in Sandage (1969), Sandage (1981), Wilson (1953), and Eggen (1964). --- id Star designation Star designation. Lowell Observatory designations (Giclas, Burnham, and Thomas 1971) are given if they exist. Otherwise, designations from the Luyten proper-motion catalogs (Luyten 1979, 1980; Luyten and Hughes 1980), the Durchmusterungen (Bonner Durchmusterung, Argelander 1859-62, Kuestner 1903, Schoenfeld 1886; Cordoba Durchmusterung, Thome 1892-1932; Cape Photographic Durchmusterung Gill and Kapteyn 1895-1900), or the Selected Area catalogs are given. --- RAh Right ascension, RA, B1950.0, hours h RAm RA, B1950.0, minutes min RAs RA, B1950.0, seconds s DE- Declination sign --- DEd Declination, Dec, B1950.0 degrees deg DEm Dec, B1950.0, minutes arcmin DEs Dec, B1950.0, seconds arcsec glon Galactic longitude deg glat Galactic latitude deg V V magnitude UBV data taken from Sandage and Kowal (1986). mag B-V B-V color mag U-B U-B color mag pmRA Annual proper motion, RA, B1950.0 The adopted proper motions have been averaged from the Lowell and Luyten catalogs, the latter proper motions in r and theta being converted to proper motions in right ascension and declination via the following relations: pmRA = pm(r)*sin(theta) pm(Dec)= pm(r)*cos(theta) arcsec/a pmDE Annual proper motion, Dec, B1950.0 arcsec/a phi Parallactic angle The angle between the equatorial and galactic coordinate systems (see Smart 1968, pp. 17-19). deg pm_lon Annual proper mot., long., B1950.0 The galactic proper motions, pm_lon and pm_lat, are calculated from the equatorial motions and the parallactic angle (phi): pm_lon = pmRA*cos(phi) + pmDE*sin(phi) pm_lat = -pmRA*sin(phi) + pm_DE*cos(phi) arcsec/a pm_lat Annual proper motion, lat., B1950.0 arcsec/a RV Radial velocity km/s obs Number of observations --- Nancy G. Roman ADC/SSDDO 1995 Jun 15 Appreciation is expressed to K. U. Ratnatunga for supplying the data file and to G. Fouts and A. Sandage for extending permission to archive and distribute the catalog from the data centers. The authors also kindly reviewed a draft version of this document prior to its release for distribution with the machine-readable catalog. This document was prepared by Wayne H. Warren Jr. and translated to ASCII in the current standard format by the undersigned. UNKNOWN UNKNOWN The machine-readable data file of New Subdwarfs. V. Radial Velocities for 889 High-Proper-Motion Stars Measured with the Mount Wilson 100-inch Reflector was received from Dr. K. U. Ratnatunga of the Space Data and Computing Division, NASA/Goddard Space Flight Center, on 8 April 1989. Permission to archive and distribute the data was subsequently obtained at different times during conversations with the authors. Minor format modifications were made to the catalog at the Astronomical Data Center in order to add plus signs to certain data, to position all signs to occur always in the same bytes, and to remove multiple spaces from between the data columns to decrease storage requirements. (A single space has been retained between each data field to facilitate reading the data.) III_144.xml U, V, W Velocity Components for the Old Disk Using Radial Velocities of 1295 Stars in the Three Cardinal Directions 3145 III/145 Radial Velocities in the Cardinal Directions U, V, W Velocity Components for the Old Disk Using Radial Velocities of 1295 Stars in the Three Cardinal Directions A Sandage G Fouts Astron. Jour. 93 592 1987 1987AJ.....93..592S Radial velocities Radial velocities are presented for 430 stars in the direction: l=180deg., b=0deg., 445 stars in the direction: l=90deg., b=0deg, and 420 stars in the direction: b=90deg. The stars were chosen from the SAO catalog to be within about 10deg of the respective cardinal directions, to be brighter than m(pg) about = 10.5, and between spectral classes A5 and K0. Except for the K0 stars, almost all are dwarfs. They were chosen to present a kinematically unbiased selection, as the intent was to understand the percentage of stars in each kinematic component of the galaxy.
Radial velocities for stars within 10deg of l=0d, b=0d Radial velocities for stars within 10deg of b=90d cat SAO or BD zone SAO in u.dat and w.dat; the BD zone followed by - in v.dat. --- num Star number The SAO number in u.dat and w.dat; the BD number in v.dat. --- comp Component --- RAh Right ascension (1950) hours h RAm Right ascension (1950) minutes min RAs Right ascension (1950) seconds s DEd Declination (1950) degrees All declinations are positive. deg DEm Declination (1950) minutes arcmin DEs Declination (1950) seconds arcsec Sp Spectral type --- v Visual Magnitude mag b Photographic magnitude mag RV Radial Velocity km/s e_RV Standard deviation of radial velocity km/s l-par Left parenthesis --- o_RV Number of measurements of radial velocity --- r-par Right parenthesis --- Radial velocities for stars within 10deg of l=90d, b=0d cat SAO or BD zone SAO in u.dat and w.dat; the BD zone followed by - in v.dat. --- num Star number The SAO number in u.dat and w.dat; the BD number in v.dat. In line 155 (47-3650) the record as it was received is appended by * 471420. This does not appear in this version or in the printed version. --- comp Component For lines 155 and 335, the BD zone was prefixed by NX. This has been changed to X in the comp column. It apparently is another star near the BD star numbered. --- RAh Right ascension (1950) hours h RAm Right ascension (1950) minutes min RAs Right ascension (1950) seconds s DEd Declination (1950) degrees All declinations are positive. deg DEm Declination (1950) minutes arcmin DEs Declination (1950) seconds arcsec Sp Spectral type --- v Visual Magnitude mag b Photographic magnitude mag RV Radial Velocity km/s e_RV Standard deviation of radial velocity km/s l-par Left parenthesis --- o_RV Number of measurements of radial velocity --- r-par Right parenthesis --- Nancy G. Roman ADC/SSDOO 1995 Sep 29 III_145.xml Studies of the Large Magellanic Cloud stellar content. III. Spectral type and V magnitudes of 1822 members 3147 III/147 Studies of LMC stellar content Studies of the Large Magellanic Cloud stellar content. III. Spectral type and V magnitudes of 1822 members J M Rousseau N Martin L Prevot E Rebeirot A Robin J P Brunet Astron. Astrophys. Suppl. Ser. 31 243 1978 1978A&AS...31..243R Magellanic Clouds This is an updated version of the original catalogue. New UBV photoelectric measurements were added from Isserstedt (1979, 1982), and Feitzinger and Isserstedt (1983). The remarks and origins of photoelectric photoelectric magnitudes are not included in this electronic version. Photoelectric data are obtained by averaging observational values made at 100 and more cm instruments (with weight=2) with ones made at 60 and less cm instruments (with weight=1). A spectral survey has been made during the period 1971 to 1975 with the ESO 40cm astrograph at La Silla, equipped with its normal prism, giving an intermediate dispersion of 95Angstroem/mm at 4026Angstroem. Long exposure plates taken directly or with an interference filter enabled us to obtain spectral types for nearly 1600 stars. In parallel, a V photographic survey has been carried out during the same period with the same astrograph and has led to the determination of V magnitudes for more that 700 stars having no previous photometric data. New spectroscopic and photometric results as well as previous photoelectric UBV values are given in the catalogue together with additional remarks concerning peculiarities of spectra, V magnitudes, and details on double and multiple systems.
The catalogue Name Identification number=1 number of the star in the following catalogues and lists: BI: Brunet et al. (1975), A&AS 21, 109 C: Ardeberg et al. (1972), A&AS 6, 249 Brunet et al. (1973), A&AS 9, 447 D: Dachs (1972), A&A 18, 271 FDA: Fehrenbach et al. (1976), A&AS 24, 379 FDS: Fehrenbach and Duflot (1970), A&A Special Suppl. no. 1, list S G: Fehrenbach and Duflot (1970), A&A Special Suppl. no. 1, list G Fehrenbach and Duflot (1973), A&AS 10, 231, list G HS: Henize (1956), ApJS 2, 315 NS: Sanduleak (1969), Contr. Cerro Tololo Int. Am. Obs. 89 OM: Martin and Rebeirot (1972), A&A 21, 329 R: Feast et al. (1960), MNRAS 121, 337 --- Bchart Number of B chart Hodge and Wright (1967) number=2 Hodge, P.W. and Wright, F.W.: 1967, The Large Magellanic Cloud, Smithsonian Publication 4699, Smithsonian Press, Washington. --- RAh Right Ascension 1975 (hours) h RAm Right Ascension 1975 (minutes) min DE- Declination 1975 (sign) --- DEd Declination 1975 (degrees) deg DEm Declination 1975 (minutes) arcmin SpType Spectral type number=3 spectral MK classification, with the terminology used by Feast et al., Ardeberg et al., and Brunet et al.; 22 non stellar objects have been classified with the usual terminology: CLUS: for clusters HII: for HII regions PN: for planetary nebulae --- r_SpType Origin of the spectral type number=4 origin of the adopted spectral type: A: Ardeberg et al. (1972), A&AS 6, 249; Brunet et al. (1973), A&AS 9, 447 C: Classifications determined from spectra obtained at the Chalonge-Divan spectrograph and published by Brunet et al. (1975), A&AS 21, 109 F: Fehrenbach et al. (1976) for the WR stars, A&AS 24, 379 P: New spectral types determined from objective prism spectra, with or without interference filter. R: Feast et al. (1960), MNRAS 121, 337 S: Sanduleak (1969), Contr. Cerro Tololo Int. Am. Obs. 89; Sanduleak (1972), A&A 17, 326 --- Vmag V photoelectric magnitude mag u_Vmag Uncertainty flag (:) on Vmag --- B-V photoelectric colour index mag u_B-V Uncertainty flag (:) on B-V --- U-B photoelectric colour index mag u_U-B Uncertainty flag (:) on U-B --- Obs Number of photoelectric measurements --- Pmag V photographic magnitude number=5 V photographic magnitude as determined from astrographic plates. A value with two decimals means a standard error less than 0.07 mag; a value with one decimal only means a standard error less than 0.15 mag; a value with one decimal and a colon means a standard error higher than 0.15 mag or one determination of low quality. mag u_Pmag Uncertainty flag (:) on Pmag number=5 V photographic magnitude as determined from astrographic plates. A value with two decimals means a standard error less than 0.07 mag; a value with one decimal only means a standard error less than 0.15 mag; a value with one decimal and a colon means a standard error higher than 0.15 mag or one determination of low quality. --- o_Pmag Number of plates used for Pmag determination --- Francois Ochsenbein CDS 1995 Sep 01 UNKNOWN UNKNOWN * 29-May-1989: this version which supersedes III/111 was provided by L. Prevot (Marseille Observatory). Compared to the original edition, UBV photoelectric data and number of measurements were recomputed. * 01-Sep-1995 (CDS): a few misaligned decimal points and uncertainty colons corrected in the catalog file. Documentation was standardized. III_147.xml The Interstellar Lines Catalogue 3148A III/148A Interstellar lines catalogue The Interstellar Lines Catalogue B Garcia Astron. Astrophys. Suppl. Ser. 89 89 1991 1991A&AS...89..159G Interstellar medium Spectroscopy catalogs catalogs: bibliography ISM: general A bibliographical catalogue of the interstellar lines has been prepared (2003 stars in our Galaxy, 86 stars in the Magellanic Clouds and 41 extragalactic objects), and 371 bibliographical references.
The Catalogue Identif Designation of the star (BD/CD/CPD/HD/HDE/ADS/Name) --- RAh Right Ascension 1950 (hours) number=1 a few objects have no position. h RAm Right Ascension 1950 (minutes) number=1 a few objects have no position. min RAs Right Ascension 1950 (seconds) number=1 a few objects have no position. s n_RAs '*' if original position given in 0.1min --- DE- Declination 1950 (sign) number=1 a few objects have no position. --- DEd Declination 1950 (degrees) number=1 a few objects have no position. deg DEm Declination 1950 (minutes) number=1 a few objects have no position. arcmin DEs Declination 1950 (seconds) number=1 a few objects have no position. arcsec n_DEs '*' if original declination given in 0.1arcmin --- Vmag V Magnitude mag u_Vmag Uncertainty flag (:) on Vmag --- Sp Spectral type --- Ref References (see table2a and table4) --- Line Interstellar line measured and type of measure number=2 type of measure indicated by 'v' = radial velocity 'w' = equivalent width 'i' = intensity 'n' = column density --- Diffuse Interstellar diffuse band observed --- l_W(K) Limit flag on W(K) --- W(K) Equivalent width of CaII K-line 0.1nm u_W(K) Uncertainty flag (:) on W(K) --- l_W(H) Limit flag on W(H) --- W(H) Equivalent width of CaII H-line 0.1nm u_W(H) Uncertainty flag (:) on W(H) --- l_W(D2) Limit flag on W(D2) --- W(D2) Equivalent width of NaI D2-line 0.1nm u_W(D2) Uncertainty flag (:) on W(D2) --- l_W(D1) Limit flag on W(D1) --- W(D1) Equivalent width of NaI D1-line 0.1nm u_W(D1) Uncertainty flag (:) on W(D1) --- Observations (references): main characteristics Ref References (see table4) number=1 this field is blank if it is a continuation. --- Line Interstellar line measured --- Diffuse Interstellar diffuse band observed --- MeasType Type of measure number=2 type of measure indicated by 'v' = radial velocity 'w' = equivalent width 'i' = intensity 'n' = column density 'gf' = oscillator strength --- Instrum Instrument used --- Det Detector used --- Disp Reciprocal dispersion used 0.1nm/mm ResolA Resolution in Angstroem 0.1nm ResolV Resolution in km/s km/s Stars Number of stars observed --- Fundamental data of Stars Catalogued HD Henry Draper Catalogue number --- HR Bright Star Catalogue (Harvard Revised) number --- RAh Right Ascension 1950 (hours) number=1 The last five stars have no position h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s n_RAs '*' if original position in 0.1min --- DE- Declination 1950 (sign) number=1 The last five stars have no position --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec GLON Galactic longitude number=1 The last five stars have no position deg GLAT Galactic latitude number=1 The last five stars have no position deg Sp Spectral type --- Vmag apparent visual magnitude mag u_Vmag Uncertainty flag (:) on Vmag --- B-V color mag Ids Other identifications --- References (from table1 and table2a) Ref Reference as in table1 and table2a --- Seq Sequence number --- Text Text of reference --- Appendix 1: Interstellar CaII and NaI Radial Velocities Id Stellar identification --- Vmag apparent visual magnitude mag u_Vmag Uncertainty flag (:) on Vmag --- Ref References (see table4) --- Line Interstellar lines measured --- Vel(CaII) CaII radial velocity km/s u_Vel(CaII) Uncertainty flag (:) on Vel(CaII) --- n_Vel(CaII) Note on Vel(CaII) number=1 the following symbols are used: C=Composite N=Not detected S=stellar line b=blended V=Variable --- Vel(NaI) NaI radial velocity km/s u_Vel(NaI) Uncertainty flag (:) on Vel(NaI) --- n_Vel(NaI) Note on Vel(NaI) number=1 the following symbols are used: C=Composite N=Not detected S=stellar line b=blended V=Variable --- System (2) --- Appendix 2: Radial Velocities data for interstellar lines published in Wilson's GCRV (1953) GCRV Wilson's GCRV number --- GC Boss's General Catalogue number --- HD Henry Draper Catalogue number --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Vmag V Magnitude mag Ref References (see table4) --- Vel Interstellar lines radial velocities km/s Notes 'GCRV' if the star presents radial velocity data for interstellar lines only in GCRV --- Francois Ochsenbein CDS 1995 Feb 20 UNKNOWN UNKNOWN * October 1989: first archived at CDS * 29-Mar-1995: version "A" - reformatted tables at CDS, corrected over 100 misalignments in tables. - table3: some stars used more than one line; all details concerning one star have been grouped into single records missing positions have been added, with the exception of the five last records - apx2: identifications neither GC nor HD were removed in HD and GC columns * 22-Sep-1997: reformatted table4 at CDS, and replaced blanks (standing for continuation lines) by their values. III_148A.xml A List of MK Standard Stars 3149 III/149 MK Standard Stars A List of MK Standard Stars B Garcia Bull. Inform. CDS 36 27 1989 1989BICDS..36...27G MK spectral classification Spectral types Stars, standard The purpose of the present work is to provide a complete list of MK standard stars, selected from the main papers related to this subject, according to the recommendations of both authors of the MK system. The catalogue provides a list of 963 standard stars, with their spectral type, luminosity, equatorial coordinates, magnitudes, colour index (B-V), and references. The magnitude and colours were taken from Mermillod (1986) UBV Photoelectric Photometry Catalogue (catalog <II/122>). In the cases without observations with the UBV catalogue, the apparent magnitude was taken from the SIMBAD data-base (SIMBAD is described at <http://cdsweb.u-strasbg.fr/Simbad.html>)
The catalogue Seq Running number --- SpTemp Spectral Temperature class --- SpLum Spectral Luminosity class --- SpPec Spectral peculiarities --- HD/BD HD or BD number --- HR Bright Star <V/50> number --- m_HR Multiplicity index on HR number --- Name Other name of the star --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s u_RAs ':' when RA originally given to accuracy of 0.1min --- DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec u_DEs ':' when DE originally given to accuracy of 0.1arcmin --- Vmag Visual magnitude mag B-V Colour index mag Refs References number=1 the references use the following symbols: C =1953ApJ...117..313J Johnson and Morgan E =1973ARA&A..11...29M Morgan and Keenan, Annual Rev. Astron. Astrophys. J : Morgan W.W., Abt H.A., Tapscott J., 1978, "Revised MK Spectral Atlas for Stars earlier than the Sun", Chicago, Yerkes Observatory K =1988BICDS..35...37K Keenan and Yorka, Bull. Inf. CDS M : Keenan P.C., McNeil R.C., 1976, "An Atlas of Spectral of the Cooler Stars: types G, K, M, S and C", Perkins Obs., Ohio State and Ohio Wesleyan Universities --- Francois Ochsenbein CDS 1996 Feb 16 UNKNOWN UNKNOWN * The original version contained two more tables with the same data sorted by right ascension and by declination. These additional tables can easily be recreated by any sort utility. * 16-Feb-1996: coordinates were originally written in several formats; the u_RAs and u_DEs columns have been introduced when tenths of (arc)minutes were converted into (arc)seconds at CDS. III_149.xml The Perkins Catalog of Revised MK Types for the Cooler Stars 3150 III/150 Perkins Revised MK Types for the Cooler Stars The Perkins Catalog of Revised MK Types for the Cooler Stars P C Keenan R C McNeil ApJS 71 245 1989 1989ApJS MK spectral classification Spectral types Stars, late-type Stars, standard The catalog contains 1054 standard stars of spectral types G0 and later (G, K, M, and a few S stars) classified on the Revised MK system at the Perkins Observatory. The revised MK system is described by Keenan (1987), and the present list is an expansion of and supersedes one published by Keenan and Yorka (1988). The spectrograms used for the classification were taken at four different observatories; hence, extensive comparisons have been made to ensure consistency between the Northern and Southern Hemispheres. The list provides a consistent set of standards in most parts of the sky and over a considerable range in magnitude. Omitted are stars of spectral types R and N, Mira variables, and stars of other groups (e.g., BY Dra variables) having spectra that are composite or so peculiar that they are not satisfactorily classified on the present system. The catalog includes star names (including Bayer and Flamsteed designations), numbers from The Bright Star Catalog, HD numbers, photoelectric V magnitudes, and spectral types.
Catalog Data Name The name or constellation letter of the star The name or constellation letter of the star preceded by + for standard type stars (* in the computer database). For fainter stars the variable star designation, or for dwarfs the number in Gliese's Catalogue (1969) is given when available, preceded by G1. The symbol G refers to Giclas' lists of faint proper-motion stars (Giclas, Burnham, and Thomas 1955-80). --- BSC The number in the Bright Star Catalogue (= the HR number) --- HD The number in the Henry Draper Catalogue --- RAh The Right Ascension in hours for the year 2000 h RAm Right Ascension in minutes min DE- sign of the Declination for the year 2000 --- DEd DEC in degrees deg DEm DEC in arcminutes arcmin Vmag1 One V magnitude for simple type star mag flag flag for Vmag1 A colon (:) indicates uncertainty, a "V" known variability. --- Vmag2 Second V magnitude for the other star type The V magnitude, taken whenever possible from the catalog of Nicolet. mag n_Vmag2 additional note for V mag A fainter magnitude if the star is variable, in which case the bright magnitude is given in Vmag. A "p" indicates that the magnitude is photographic. --- Sp The spectral type --- rem An asterisk (*) denotes that a remark will be found in the "notes.dat" file --- Notes rem Remarks --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Aug 16 UNKNOWN UNKNOWN The Revised MK system has been described by Keenan (1987). For the best-determined types, that can serve as standards, has been published by Keenan and Yorka (1988). The types were determined visually from the instruments listed in Table 1. Table 1 TELESCOPES AND SPECTROGRAMS ___________________________________________________________________ Observatory Telescope Spectrograph Scale Perkins 0.8 meter Meinel 85 A/mm Lowell 1.8 Boller & Chivens 77 Cerro Tololo 1.5 Hiltner 78 Las Campanas 0.6 Garrison 68 ------------------------------------------------------------------- In the Catalog the temperature types are generally given to a quarter of a subclass (e.g., K0, K0+, K0.5, K1-, K1), but when not all the decimal divisions of a class are counted as a subclass (as in type G). The full subclasses that we use are the following: G0, G2, G5, G8, K0, K1, K2, K3, K4, K5, M0, M1, M2, M3, M4, M5, M6, M7, M8. III_150.xml Catalogue of K Stars Towards the South Galactic Pole 3151 III/151 UBV K Stars South Galactic Pole Catalogue of K Stars Towards the South Galactic Pole K Kuijken G Gilmore Mon. Not. R. Astron. Soc. 239 605 1989 1989MNRAS.239..605K Galactic pole, south Stars, K-type B and V photographic photometry is collected for approximately 2000 stars near the south galactic pole with 0.8<B-V<1.20; v<19.0, and B<20.06. Velocities with respect to the local standard of rest are provided for approximately 500 K dwarfs and K giants.
UK Schmidt photometric data - south gal. pole ID Star number --- RAh Right ascension hours (1950) h RAm Right ascension minutes (1950) min RAs Right ascension seconds (1950) s DE- Sign of declination --- DEd Declination degree (1950) deg DEm Declination minute (1950) arcmin DEs Declination second (1950) arcsec V V magnitude mag e_V Mean error of V e_V and e_B refer to the rms scatter of the different plates' measurements, not the errors in the mean e_B-V refers to the error on the mean mag B B magnitude mag e_B Mean error of B e_V and e_B refer to the rms scatter of the different plates' measurements, not the errors in the mean e_B-V refers to the error on the mean mag B-V B-V color All stars with 0.80 < B-V < 1.20, V < 19.0, B < 20.06 are listed. mag e_B-V Mean error of B-V color e_V and e_B refer to the rms scatter of the different plates' measurements, not the errors in the mean e_B-V refers to the error on the mean mag Las Campanas Plates photometric data ID Star number --- L The letter L --- RAh Right ascension hours (1950) h RAm Right ascension minutes (1950) min RAs Right ascension seconds (1950) s DE- Sign of declination --- DEd Declination degree (1950) deg DEm Declination minute (1950) arcmin DEs Declination second (1950) arcsec V V magnitude mag e_V Mean error of V e_V and e_B refer to the rms scatter of the different plates' measurements, not the errors in the mean e_B-V refers to the error on the mean mag B B magnitude mag e_B Mean error of B e_V and e_B refer to the rms scatter of the different plates' measurements, not the errors in the mean e_B-V refers to the error on the mean mag B-V B-V color All stars with 0.80 < B-V < 1.20, V < 20 are listed. mag e_B-V Mean error of B-V color e_V and e_B refer to the rms scatter of the different plates' measurements, not the errors in the mean e_B-V refers to the error on the mean mag Spectral data for K dwarfs, 8-plate photometry Spectral data for K giants ID Star number Where given, ID refers to ID in table8.dat. --- RAh Right ascension hours (1950) h RAm Right ascension minutes (1950) min RAs Right ascension seconds (1950) s DE- Sign of declination --- DEd Declination degree (1950) deg DEm Declination minute (1950) arcmin DEs Declination second (1950) arcsec V V magnitude mag B-V B-V color mag V-lsr Velocity w/respect to local std of rest km/s e_V-lsr Uncertainty of V-lsr? e_V-lsr refers to the rms scatter of the different plates' measurements, not the errors in the mean km/s Spectral data for K dwarfs, 4-plate photometry ID Star number --- i The letter i --- RAh Right ascension hours (1950) h RAm Right ascension minutes (1950) min RAs Right ascension seconds (1950) s DE- Sign of declination --- DEd Declination degree (1950) deg DEm Declination minute (1950) arcmin DEs Declination second (1950) arcsec V V magnitude mag B-V B-V color mag V-lsr Velocity w/respect to local std of rest km/s e_V-lsr Uncertainty of V-lsr? e_V-lsr refers to the rms scatter of the different plates' measurements, not the errors in the mean km/s Julie Anne Watko SSDOO/ADC 1996 Apr 10 III_151.xml An Atlas of Stellar Spectra between 2.00 and 2.45 micrometers 3153 III/153 An Atlas of Near Infrared Stellar Spectra An Atlas of Stellar Spectra between 2.00 and 2.45 micrometers K A Arnaud G Gilmore C A Collier Mon. Not. Roy. Astron. Soc. 237 495 1989 1989MNRAS Spectra, infrared Spectrophotometry The atlas represents a collection of spectra in the wavelength range 2.00 to 2.45 micrometers having a resolution of approximately 0.02 micrometers. The sample of 73 stars includes a supergiant, giants, dwarfs, and subdwarfs with a chemical abundance range of about -2 to +0.5 dex.
An Atlas of Stellar Spectra between 2.00 and 2.45 micrometers contains digital spectra for a sample of 73 stars of various temperature classes of F and later, most luminosity classifications, and a range of abundances. A majority of the spectra were obtained with the UKIRT, while some observations were collected with the Mount Hopkins MMT. The UKIRT provided a 59-point spectrum from 2.004 to 2.451 micrometers and the MMT gave a 30-point spectrum from 2.001 to 2.431 micrometers. This documentation should be used only to supplement the information contained in the source reference, which should be consulted for details regarding the impetus for the work, the selection of standard stars, the observational procedures, and the technique of data reduction. The source reference also contains a full listing of the observed stars and a table of flux standards used. Graphical presentations of all spectra are also given in the body of the paper, while the digital spectra are listed on a microfiche card accompanying the journal issue. (Note: The labels on the two microfiche cards in the issue are reversed.) In any case, the published paper should be consulted by all users of the machine-readable data.
The catalog lambda Wavelength in micrometers um flux Flux normalized to unity at lambda. = 2.15 micrometers --- e_flux Fractional error of flux --- Nancy G. Roman SSDOO/ADC 1995 Mar 16 Appreciation is expressed to Dr. Keith Arnaud for supplying the digital spectra and for reviewing a draft copy of the present document before it was finalized for distribution with the machine-readable atlas. This document has been adapted from the version prepared by Wayne Warren. UNKNOWN UNKNOWN The machine-readable version of An Atlas of Stellar Spectra between 2.00 and 2.45 micrometers was received on 3 November 1989 via SPAN network transfer from Dr. K. A. Arnaud of the Laboratory of High Energy Astrophysics at the NASA Goddard Space Flight Center. Minor changes were made to some of the header records in order to make the spacing uniform; otherwise, the archived and distributed data are exactly as received. III_153.xml Radial Velocities in Three Fields Along the Southern Galactic Equator 3154 III/154 Radial Velocities Along Southern Galactic Equator Radial Velocities in Three Fields Along the Southern Galactic Equator J Denoyelle Astron. Astrophys. Suppl. 70 373 1987 1987A&AS...70..373D Radial velocities Regional catalog This catalog contains a list of radial velocities, obtained from "Grand Prisme Objectif" (GPO) plates from La Silla, for 764 stars in three fields in the Vela-Carina region of the galaxy. The method of reduction is described in Duflot and Fehrenbach (1955) and Duflot et al. (1958).
Catalogue of radial velocities field Number of the field --- ID Running number of the star --- CPDzone Cape Photographic Durchmusterung zone --- CPDnum Cape Photographic Durchmusterung number --- RAh Right Ascension (eq. 1950) hours h RAm Right Ascension (eq. 1950) minutes min RAs Right Ascension (eq. 1950) seconds s DE- Declination (eq. 1950) sign --- DEd Declination (eq. 1950) degrees deg DEm Declination (eq. 1950) arcminutes arcmin RV_GPO GPO radial velocity km/s nplates Number of plates --- e_RV_GPO Mean error of RV_GPO km/s RV_pub Radial velocity previously published km/s age Class of age of the etalon used 1 = young star 2 = less young 3 = intermediate --- rem Remark about dispersion * = velocity is larger than twice the dispersion ** = velocity is larger than three times the dispersion. --- Julie Anne Watko SSDOO/ADC 1996 Aug 21 III_154.xml A General Catalog of Cool Galactic Carbon Stars, 2nd edition 3156 III/156 Cool Galactic Carbon Stars, 2nd Edition A General Catalog of Cool Galactic Carbon Stars, 2nd edition C B Stephenson Publ. Warner & Swasey Obs., 3, No. 2 ??? ??? 1989 1989PW&SO...3...53S Stars, carbon The catalog is intended to list all 5987 cool carbon stars having known positions of at least roughly the precision of The Henry Draper Catalogue. Cool carbon stars are defined as stars whose spectra at low dispersion (say a resolution no better than 1-2 angstroms) are known to show bands of the Swan system of the C2 molecule; or, if the spectral region of the Swan system is inadequately observed, they show the red or infrared bands of CN in strength adequate to infer that the Swan bands almost certainly would be seen if their presence could be tested. The closing date for literature search was 1989 June 30, defined by literature received in the author's library by that date. The catalog includes equatorial coordinates (B1900.0); photographic, visual, and infrared magnitudes; spectral types, galactic coordinates, and cross identifications to various other designation systems.
Data for 5987 carbon stars CGCS Catalog running number --- RAh Right Ascension B1900 (hours), see PosFlag h RAm Right Ascension B1900 (minutes) min RAs Right Ascension B1900 (seconds) s DE- Declination sign --- DEd Declination B1900 (degrees), see PosFlag deg DEm Declination B1900 (minutes) arcmin DEs Declination B1900 (seconds) arcsec Pmag Photog. magnitude, numerical mag u_Pmag Colon for uncertainty in Pmag --- Vmag Visual magnitude, numerical mag u_Vmag Colon for uncertainty in Vmag --- IRmag Infrared magnitude, numerical mag u_IRmag Colon for uncertainty in IRmag --- GLON galactic longitude, l(II) deg GLAT galactic latitude, b(II) deg l_bmag Limit on bmag --- bmag b magnitude mag l_vmag Limit on magnitude vmag --- vmag v magnitude mag n_vmag uncertain; v/V=variable; r/R=remark --- imag i magnitude mag n_imag Magnitude flag on i --- SpType Spectral types string --- Names Designations string --- Rem Remarks string --- PosFlag Position (coordinates) Precision flag The following table lists the value of Position Precision flag and gives the corresponding format used in the printed (published) catalog. PosFlag Printed Format 0,1 HH MM SS.S +dd mm ss 2 HH MM SS +dd mm.m 3 HH MM.M --- Notes to the catalog CGCS Catalog running number --- cont The '+' indicates incomplete record --- rem comments --- Stars that have been published as Carbon, but probably or definitively are not. RAh RA hours (B1900) h RAm RA in minutes (B1900) min RAs RA in seconds (B1900) s DE- Sign of Declination (B1900) --- DEd Dec degrees (B1900) deg DEm Dec in arcminutes (B1900) arcmin DEs Dec in arcseconds (B1900) arcsec cont The '+' indicates incomplete record --- SpSource Spectral Sources or Designations --- rem Remarks --- Notes for Table 2 RAh RA hours (1900) The notes to Table 2 (table2.dat) are referenced by right ascension. h RAm RA in minutes (1900) min RAs RA in seconds (1900) s cont The '+' indicates incomplete record --- rem Remarks --- C.-H. Joseph Lyu Hughes STX/NASA 1996 Jun 19 The ADC Intro file provided by C. B. Stephenson (1989) together with the description file by Wayne H. Warren (1991) were used to create this ReadMe file. UNKNOWN UNKNOWN * Star #364 was found to have an incorrect declination in both the published and machine-readable catalogs. The latter has been corrected in both declination and galactic coordinates...WHW/ADC 3/1991. * Star #4942 was erroneously typed 4972 (FO/CDS, 1997/01) III_156.xml An Ultraviolet atlas of Quasar and Blazar Spectra 3157 III/157 AN ULTRAVIOLET ATLAS OF QUASAR AND BLAZAR SPECTRA An Ultraviolet atlas of Quasar and Blazar Spectra A L Kinney R C Bohlin J C Blades D G York Astrophys. J. Suppl. Ser. 75 645 1991 1991ApJS Atlases Galaxies, Seyfert QSOs Spectra, ultraviolet This atlas contains the ultraviolet spectra of 70nquasars, blazars, and Seyfert 1 galaxies that were produced by combining over 100 low resolution spectra from the International Ultraviolet Explorer (IUE) data archive. The spectra have been extracted with an optimal algorithm (see Kinney et al. 1991) and co-added to produce spectra with the best possible signal-to-noise ratio.
The spectra file currently present in this directory are the digital versions of the spectra that were extracted and co-added for the Ultraviolet Atlas of Quasar and Blazar Spectra, 1991 (reference above) The files contain the optimally extracted data which are described in "Weighted Slit Extraction of Low Dispersion IUE spectra. The optimal extraction is described in A. L. Kinney, R. C. Bohlin, and J. D. Neill 1991, PASP, 103, 694. Each co-added spectrum consists of the wavelength, quality flag, gross flux, background flux, gross flux divided by time, absolutely calibrated net flux, exposure time, and sigma. Details from the headers which formerly prefixed each spectrum are in headers.dat. A third file (objects.dat) is also available, which contains information from Table 1 in the published paper: IAU and alternate designations, redshift (z), V magnitude, object type, E(B-V), galactic longitude and latitude, and number of spectra. The file formats are mostly self explanatory. THE S-AP NOMENCLATURE INDICATES THE SPECTRA THAT ARE NORMALIZED IN FLUX TO THE L-AP SET (USUALLY ONE SPECTRUM, see paper for a more detailed explanation) AND DOES *NOT* MEAN THAT THE SPECTRA WERE OBTAINED IN THE SMALL ENTRANCE APERTURE. The camera numbers of co-added spectra are listed. Each co-added spectrum has 8 columns of ASCII numbers with the titles.
The data for 0007+106 The data for 026+129 The data for 044+030 The data for 119-013 The data for 121-590 The data for 215+015 The data for 219+428 The data for 312-770 The data for 316+413 The data for 405-123 The data for 430+052 The data for 513-002 The data for 521-365 The data for 537-441 The data for 637-752 The data for 735+178 The data for 742+318 The data for 754+100 The data for 804+761 The data for 844+349 The data for 851+202 The data for 946+301 The data for 955+326 The data for 957+561 The data for 004+130 The data for 011+250 The data for 101+384 The data for 115+080 The data for 116+215 The data for 119+120 The data for 133+704 The data for 146-037 The data for 148+549 The data for 156+295 The data for 202+281 The data for 211+143 The data for 219+755 The data for 225+317 The data for 226+023 The data for 229+204 The data for 241+176 The data for 253-055 The data for 302-102 The data for 317+277 The data for 351+640 The data for 411+442 The data for 426+015 The data for 512+370 The data for 553+113 The data for 613+658 The data for 630+377 The data for 634+706 The data for 641+399 The data for 652+398 The data for 700+518 The data for 704+608 The data for 721+343 The data for 807+698 The data for 821+643 The data for 833+326 The data for 005-489 The data for 128-123 The data for 130+099 The data for 135-147 The data for 155-304 The data for 200+420 The data for 223-052 The data for 251-178 The data for 308+098 The data for 1700_64 ID Identification --- LAM Wavelength m-10 EPS Quality flag --- GROSS Gross flux --- BKG Background flux --- NET/TIME Gross-background divided by time --- ABNET Absolute calibrated net flux mW/m2/m-10 TIME Exposure time s SIGMA (Example: 2.1 = 210 percent) The SIGMA is the RMS scatter among the co-added spectra at each wavelength. In qso70.dat, a zero has been added to byte 80 to permit reading this file with the same format as that for the other files. This zero should be ignored. --- Details on objects included IAU IAU designation --- alt Alternate designation --- z Redshift z km/s n_z a=Redshift from Veron+Veron 19827-31 --- V V magnitude mag type Type QSO (quasar) SY1 (Seyfert type I) BLZ (blazar) --- E E(B-V) mag glon galactic longitude deg glat galactic latitude deg no Number of spectra in each atlas. --- Nancy G. Roman ADC/SSDOO 1995 Sep 01 The undersigned thanks Ralph Bohlin for providing this version of the catalog and substantial advice. She also thanks Arthur Davidson for providing the information on 1700+643. UNKNOWN UNKNOWN The file objects.dat was added by the CDS. The file headers.lst is best read as a straight ASCII file. Contact Anne Kinney (KINNEY@stsci.edu) for additional information. III_157.xml Catalogue de Vitesses Radiales Moyennes Stellaires 3161 III/161 Averaged Stellar Radial Velocities Catalogue de Vitesses Radiales Moyennes Stellaires M Barbier-Brossat Astron. Astrophys. Suppl. 80 67 1989 1989A&AS...80...67B III/21 : General Catalogue of Stellar Radial Velocity (Wilson, 1953) III/47 : Catalogue of Stellar Radial Velocities (Evans, 1967) Batten A.H., Flechter J.M., Mann P.J., 1978, Publ. Dominion Astrophys. Obs. 15, 121 Evans, D.S., 1978, "Catalog of Stellar Radial Velocities" (unpublished) Wilson, R.E., 1953, "General Catalog of Stellar Radial Velocities", Carnegie Institution of Washington, Pub. 601, Washington, D.C. Radial velocities This catalog contains means of measurements of radial velocities of galactic stars. The data supplement the catalogs of Wilson (1953) <III/21> and Evans (1978) <III/47> with observations published through December 1980. There are new mean velocities for 6023 stars with new radial velocity data; more than 4500 of these stars are not in the earlier catalogs. A weighting scheme was used to form the mean velocities with data from cross-correlation spectrometers given highest weight and low dispersion (less than 100 A/mm) spectra given lowest weight. No systematic zero-point corrections were made but observations were taken from the literature only if they were standardized to the IAU or Wilson (1953) systems.
The catalogue Name Identification of the star: HD number if existing, indicated by blank columns 1-2; BD, CP or CD otherwise --- Alias Other designation --- RAh Right Ascension 1950 (hours) number=1 The coordinates are those published by the author when existing; they are otherwise taken from the C.S.I. (Catalogue of Stellar Identifications, Strasbourg Data Center), or derived from other sources. h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin n_Mag '*' indicates a B magnitude --- Mag V magnitude, or B when column 49 is '*'. mag u_Mag A colon (:) denotes an inaccurate magnitude; 'v' indicates a variable star (the Mag column is then blank) --- Sp Spectral type, either from the authors, or from the C.S.I. <V/26> --- RV Mean Radial Velocity (km/s). number=2 The radial velocity has no fractional part when the mean error is larger than 3.70 km/s. For binaries (byte 81 = 'O'), we provide the systemic velocity of the most recently published orbit calculation. For standard stars (byte 81 = 'S'), we provide the most recent value recommended by I.A.U. This value will be regularly updated. km/s e_RV Mean error in km/s; blank when a remark ('O' or 'S') exists in byte 81. (see comments in cols 68-74) km/s n_RV Remark as: O = ORB (spectroscopic binary) ; S = STND (IAU standard star) --- o_RV Number of measurements used to derive the Mean Radial Velocity --- Nrefs Number of references used, including Wilson (1953) and Evans (1978) --- Notes Notes as: W = the star has a velocity in Wilson (1953) ; E = the star has a velocity in Evans (1978) ; B = the star has a velocity in Batten (1978) --- ref1 Reference --- ref2 Reference --- ref3 Reference --- ref4 Reference --- ref5 Reference --- The references (cols 92-116 of file main) Ref Reference code (the integer part corresponds to a journal, and the fractional part to the column, page and year) --- Journal Abbreviation of the journal name or publication --- Vol Volume number --- Comma --- Page Page number --- [-] Dash --- Year Publication year yr Title Full publication title --- Francois Ochsenbein CDS 1995 Nov 02 UNKNOWN UNKNOWN * 04-Jul-1992: first archived * 10-Jun-1994: standardized document, reformatted columns of RV and Mag (comments pushed to columns 81 and 55) * 02-Nov-1995: Description (from ADC, NASA/Goddard) added III_161.xml A Master Catalogue of Equivalent Widths of the Interstellar 217 nm Band 3164 III/164 Cat of Eq Widths of Interstellar 217 nm Band A Master Catalogue of Equivalent Widths of the Interstellar 217 nm Band C Friedemann CDS Inf. Bull., No. 40, p. 31 ??? ??? 1992 1992BICDS..40...31F Equivalent widths Interstellar medium (from CDS Inf. Bull. 40, 31) The main task of the catalogue consists in a comprehensive collection of equivalent widths of the 217 nm band derived from both spectrophotometric and filterphotometric measurements obtained with TD-1, OAO-2 and ANS satellites. These data concern reddened O, B stars with color excesses E(B-V) >= 0.02 mag.
The relative errors amount to about {delta}A/A = +/- 0.10, {delta}B/B = +/- 0.02 and {delta}C/C = +/- 0.03.
Catalog Data ID HD or BD number --- E(B-V) E(B-V) Color excess mag lambda_c Central wavelength of the 2200 band (A) A A A parameter (defined in the publication) --- B B parameter (defined in the publication) --- C C parameter (defined in the publication) --- W Equivalent width (A) A negative value indicates that a flat minimum instead of a maximum has been found in the extinction curve in the wavelength region of the 2200 A band. In these cases W was computed with lambda_c = 2182 A. A N Number of observations --- rem Remarks O: Filterphotometry from OAO-2 J: Spectral flux data from LSR of IUE C: The wavelength of the centre of the absorption band has been fixed to the average value lambda_c = 2182 A because the searching procedure for lambda_c had led to a value lambda_c outside the presumed interval from 2182 - 2228 A. The parameters A B C and W were computed with the average value lambda_c = 2182 A.D D: within one arcminute of the pointing position at least two stars are present (Wesselius et al. 1982) V: Ultraviolet ANS data (Wesselius et al., 1982) indicate variability --- Julie Anne Watko SSDOO/ADC 1996 Jun 04 UNKNOWN UNKNOWN The master catalogue contains all relevant data sets published earlier (see Dorschner, 1984; Friedemann, 1987; Friedemann, 1988) by the CDS and should replace them. III_164.xml A New Library of Stellar Optical Spectra 3166 III/166 A New Library of Optical Spectra A New Library of Stellar Optical Spectra D R Silva M E Cornell Astrophys. J. Suppl. 81 865 1992 1992ApJS...81..865S Spectrophotometry Newly acquired and previously published data have been combined to form a new digital optical library intended primarily for use in empirical population synthesis. Stellar data for a large number of individual stars were acquired during seven observing runs between December 1988 and May 1989. An effort was made to observe, primarily, stars with TZG parameters derived from stellar atmosphere models of high dispersion data. Observations of photometric calibration stars were made during each run, but absolute calibrations were not attempted. Composite spectra from different observations of each star were formed by multiplicatively scaling the individual sub-spectra and averaging. The resultant composite spectra were normalized to 100 at 5450A. Next, the effects of interstellar reddening were removed. Intensities in the spectral regions most affected by telluric absorption were set to zero. Finally, stars with similar TZG parameters and similar overall spectral characteristics were averaged to form the individual spectra in the library, also normalized to 100 at 5450A. Table 1 lists the individual types averaged to form each of the 72 entries in the catalog. The prefixes R and W refer to strong- and weak-line stars, respectively. In the reference a list of observed stars with complete spectral coverage is given, a list of spectra used for creating the composite spectra, and a table of synthesized versus catalog UBV colors. Silva and Cornell have compiled a new digital optical stellar spectra library, consisting of intensities at 5A intervals between 3510A and 8930A for 72 different spectral types. These types range from O to M and luminosities range from I to V. Some weak-line and strong-line spectra are also included. The intensities are in ergs/A, normalized to 100 at 5450A.
O5.5V - included types O7.5V, O8V,B0V B3V, B4V B6V A1V, A2V, A2V, A3V A5V, A6V, A7V A8V A9V, F0V F6V, F7V F8V, F9V G1V, G2V, G2V G6V, G7V, G7V, G8V, G8V K2V, G9V, G9V,K0V,K0V,K0V K4V K5V M2-V M4.5VE F0M F3IV F8V, F8III-IV, F9IV G2V, G2IV G5IV G8IV O7.5III, O8.5III, O9.5III,B1III B5III B9III A3III A6III, A8III, F0III F4III, F6III, F7III G0III, G2III, G4III G5III-IV, G6III, G9III K0III, G8III, K0III, K0III K2III, K2III K4III, K4III K7III M0.5IIIab, M1III, M1.5IIIb M3III, M3-III, M3+III, M3III M4III, M4.5III M4.5III, M5III M5-III M6-7SIII O6IF, O5IF O8I B1IA B5IA, B3I B8IA A0IB, A3IA A7I, A9I F0IB, F3I F7I G0IA, G1I K1IB, K2I K5I M0.5IIb M3IIb C0 G5V G8V K0V, K0V, K0V, K0V B9P, B9III,B9PSI, B9III F8V K2IIICN2 K3IIICN1, K3IIICN2, K3III K3IB, K3IAB-IB GOV, G1V G1V, G1V, G2V, G2V G5V, G5V G7V, G7V, G7V, G7V G8V, G9V, G9V, K0V, K0V, K0V, K0V F5V F9V A2VI wavel central wavelength for each pixel nm I normalized intensity to 100 at 545.0 nm The intensities have been normalised to a value of 100 at a wavelength of 5450 Angstrom. J/m N.P.M. Kuin NASA/SSDOO/ADC 1995 Apr 25 UNKNOWN UNKNOWN The data were received by the ADC as one large file. The individual spectra were extracted and put in individual files. A wavelength scale was appended explicitly to each file. III_166.xml An Atlas of Ultraviolet Spectra of Starforming Galaxies 3167 III/167 Atlas of UV Spectra of Starforming Galaxies An Atlas of Ultraviolet Spectra of Starforming Galaxies A L Kinney R C Bohlin D Calzetti N Panagia R F G Wyse Astrophys. J. Suppl. 86 5 1993 1993ApJS...86....5K Atlases Galaxies, IR Galaxies, Markarian Galaxies, nearby Galaxies, optical Galaxies, radio Galaxies, Seyfert Galaxies, spectra Galaxies, UV-excess Galaxy catalogs Spectra, ultraviolet This catalog contains the co-added spectra from "An Atlas of Ultraviolet Spectra of Starforming Galaxies" (AUVSSG). Data for this atlas were obtained from the IUE archives and include spectra from the short wavelength prime (SWP, camera 3), long wavelength prime (LWP, camera 1), and long wavelength redundant (LWR, camera 2) cameras. Only large aperture (10 arcsec x 20 arcsec rectangular slit) spectra were used. An optimal extraction technique was used to extract the spectra from the spatially resolved IUE data. See Kinney et al. (1991a) for a discussion of the optimal extraction technique and AUVSSG for a discussion of the extraction and calibrations used in this atlas. A previous atlas of Kinney et al. 1991b was also generated using similar techniques. Note that the archival data for this catalog were processed with the IUE Spectral Image Processing System (IUESIPS) (Turnrose and Thompson 1984). Structure: The Files as a Whole The holdings for "An Atlas of Ultraviolet Spectra of Starforming Galaxies" consist of three files. Two versions of Table 1 from AUVSSG are available. One version is in TEX format. A second ASCII format version of Table 1 is contained in a single fixed-block file of 143 146-byte records. The atlas spectral data are contained in a single fixed-block file of 177600 78-byte records. Detailed descriptions of some of the fields in the files are given in the following sections.
This atlas contains the ultraviolet spectra of the central regions of 143 spiral, irregular, blue compact, Seyfert 2, and starburst galaxies, which were produced by combining 387 low resolution spectra from the International Ultraviolet Explorer (IUE) data archive. The spectra have been extracted with an optimal algorithm and co-added to produce spectra with the best possible signal-to-noise ratio. The holdings for this catalog include three files: One file contains the atlas spectral data in ASCII format, and two files (ASCII and TEX format) contain Table 1 from Kinney, Bohlin, Calzetti, Panagia, and Wyse (1993). Table 1 lists summary information about each galaxy including the figure number, galaxy name, morphological type, activity class, recession velocity, apparent magnitude, absolute magnitude, E(B-V), galactic longitude and latitude, right ascension, declination and other names. For each galaxy the atlas spectral data file contains the following columns: wavelength, IUE quality flag (Epsilon), gross flux, background flux, net flux divided by exposure time, absolute calibrated net flux, exposure time, and sigma. The atlas spectral data file consists of 177600 78-byte records and the ASCII version of Table 1 has 143 146-byte records.
ASCII version of Table 1 ref Figure number or activity class reference --- SWPnum Number of SWP spectra --- LWnum Number of LWP or LWR spectra --- name Galaxy name The names, cross-identifications, coordinates, and some of the morphological types are taken first from RSA or from the literature, and otherwise come from the NASA Extragalactic Database (NED). The morphological type follows, where possible, the classical Hubble classification. Specific symbols are Am. = amorphous, Comp. = compact, Cl. Irr. = clumpy irregular, 2-nuc. = presence of two nuclei. --- MType Morphological type --- class Activity class --- vH recession velocity The recession velocity (vH) and the apparent magnitude (BT) are from "The Revised Shapley-Ames Catalogue" when no marks are shown; vH is the heliocentric velocity; BT is the apparent magnitude in the BT system of the RC2 ("Second Reference Catalogue of Bright Galaxies"); MB is the absolute magnitude calculated from an apparent magnitude corrected for galactic and internal absorption and from a recession velocity reduced to the centroid of the Local Group (cfr. RSA). km/s Note_1 Note 1 Note 1, Note 3, and/or Note 4: An asterisk following a value of vH, BT, or MB means the following: vH and BT correspond to the heliocentric velocity and to the uncorrected apparent magnitude from "The Third Reference Catalogue of Bright Galaxies" (RC3); vH is the V21 or the Vopt when the first is not available (the difference between the two is in general small). The absolute magnitude MB is obtained from RC3 using the velocity reduced with respect to the Galactic Standard of Rest, vGSR, the apparent magnitude corrected for galactic and internal absorption, BoT, and assuming H0 = 50 km/s/Mpc. For recession velocities between 500 and 3000 km/s MB has been calculated with the usual formula after checking that it is not near a cluster. For v > 3000 km/s the formula has been applied without problem. Redshift corrections were applied for v > 10,000 km/s. For galaxies belonging to a cluster MB has been obtained from BoT (RC3) and with the assumed distance being the distance of the cluster. --- BT apparent magnitude --- Note_2 Note 2 Note 2 and/or Note 5: Other notation is as follows: p-When BT is not available from RC3, the photographic magnitude has been reported; o-This marks galaxies with redshift in the range 500-3000 km/s, but not belonging to a cluster; m-This marks the distances calculated through the distance modulus; a-BT or corrections to derive BoT have been taken from r1; b-BoT have been taken from r2; c-Galaxies for which BT or vH or both have been taken from NED since they are not reported in RSA or in RC3; the same values have been used to calculate an approximate value for MB. The symbol indicates also an approximate MB for galaxies with both vH and BT from RC3 but without the extinction corrected BoT. Spectral Atlas File The information for each galaxy consists of a header plus the co-added spectra and is separated from the next object by a blank line (record) of 78 bytes. Each co-added spectrum is preceeded by a header containing the object number, object name, IUE camera(s), and image number(s) that were used to form the co-added spectrum. A sample header is given below. The first line contains the target number and the object name. The next line gives the total number of individual spectra that were used to form the co-added spectrum from the SWP (camera 3) camera. The next four lines give the individual image number(s) of the spectra, used to form the co-added SWP spectrum. Note that the S-AP nomenclature indicates the spectra are normalized in flux to the L-AP set of spectra and does NOT mean that the spectra were obtained in the small aperture. A second group of five lines may also be given in the header for the long wavelength camera (either the LWP [camera 1] or LWR [camera 2]). The first byte in each line (record) in the header is blank. In the example below only one large aperture SWP and one large aperture LWP image were used to form the spectrum of 1050+04. ### 1 1050+04 SUM OF 1 L-AP & 0 S-AP IMAGES CAMERA 3 L-AP: 18807 L-AP: S-AP: S-AP: SUM OF 1 L-AP & 0 S-AP IMAGES CAMERA 1 L-AP: 1769 L-AP: S-AP: S-AP: LAM EPS GROSS BKG NET/TIME ABNET TIME(sec) SIGMA The header is immediately followed by the co-added spectral data. Each co-added spectrum consists of eight columns of ASCII numbers with the column headings as described in Table 1. Bytes Units Format Item 2- 7 A F6.1 Wavelength 9-14 F6.0 Epsilon 16-23 FN F8.0 Gross flux 25-32 FN F8.0 Background flux 36-42 FN/sec F7.2 Net flux/time 44-53 erg/(cm*cm sec A) E10.3 ABNET 55-63 sec F9.2 Exposure time 67-73 F7.4 Sigma Table 2: Catalog Record Format Notes to Table 2 Epsilon: IUE data quality flag. See Kinney et al.(1991a) for discussion of how the epsilon values were determined for the optimal extraction algorithm. Gross flux: The gross flux is given in IUE Flux Number (FN) units. Background flux: The background flux is given in IUE Flux Number (FN) units. Net flux/time: The net flux (gross-background)/time. ABNET: Absolutely calibrated net flux. Sigma: Sigma represents the error in the mean as estimated from the IUE noise models constructed by the authors. Sigma is given in percent (i.e., 2.1 = 210%). --- Note_3 Note 3 --- MB absolute magnitude mag Note_4 Note 4 --- Note_5 Note 5 --- E(B-V) E(B-V) The reddening E(B-V) from our Galaxy is from Burstein, D. and Heiles, C. 1984, ApJ Supp., 54, 33. The activity classification is as follows: BCG and BCDG are, respectively, blue compact galaxies and blue compact dwarf galaxies (where a blue compact galaxy is considered to be a dwarf if it has MB fainter than -20); Sy2 are Seyfert 2 galaxies; SB nuc. are galaxies experiencing a starburst in their nuclei; Hs are hotspot galaxies; Lin are LINERs; HII are galaxies with spectra typical of an HII region. The criterion for defining the class is not based on physical considerations but comes from the literature, where the most widely accepted classification has been used for each galaxy. The first column gives the figure number for galaxies treated individually in this paper. If no figure is given, a reference for the activity classification is given as listed below: (r1) Thuan, T. X. and Martin, G. E. 1981, ApJ, 247, 823, (BCDG). (r2) Gordon, D. and Gottesman, S. T. 1981, AJ, 86, 161, (BCG). (r3) Mazzarella, J. M. and Balzano, V. A. 1986, ApJ Suppl., 62, 751, (Mrk). (r4) Kollatschny, W. and Fricke, K. J. 1986, IAU Symp. no. 121, p. 377. (r5) Phillips, M. M., Charles, P. A., and Baldwin, J. A. 1983, ApJ, 266, 485. (r6) Lamb, S. A., Gallagher III, J. S., Hjellming, M. S., and Hunter, D. A. 1985, ApJ, 291, 63. (r7) Zamorano, J. and Rego, M. 1986, A&A, 170, 31. (r8) Joseph, R. D., Meikle, W. P. S., Robertson, N. A., and Wright, G. S. 1984, MNRAS, 209, 111. (r9) Keel, W. C. 1983, ApJ Suppl., 52, 229. (r10) De Robertis, M. M. and Osterbrock, D. E. 1986, ApJ, 301, 727. (r11) Huchra, J. P., Wyatt, W. F., and Davis, M. 1982, AJ, 87, 1628. (r12) Heckman, T. M., Van Breugel, W., Miley, G. K., and Butcher, H. R. 1983, AJ, 88, 1077. (r13) Moorwood, A. F. M. and Oliva, E. 1988, A&A, 203, 278. (r14) Heckman, T. M. 1980, A&A, 87, 152. (r15) Osterbrock, D. E. and Cohen, R. D. 1982, ApJ, 261, 64. (r16) Veron-Cetty, M.-P. and Veron, P. 1986, A&A Suppl., 65, 241. (r17) Lamb, S. A., Bushouse, H. A., and Towns, J. W. 1989, BAAS, 21, 1163. (r18) Keel, W. C., Kennicut, R. C. Jr., Hummel, E., and Van der Hulst 1985, AJ, 90, 708. (r19) Netzer, H., Kollatschny, W., and Fricke, K. J. 1987, A&A, 171, 41. mag GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination Sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec names Other_names The names, cross-identifications, coordinates, and some of the morphological types are taken first from RSA or from the literature, and otherwise come from the NASA Extragalactic Database (NED). The morphological type follows, where possible, the classical Hubble classification. Specific symbols are Am. = amorphous, Comp. = compact, Cl. Irr. = clumpy irregular, 2-nuc. = presence of two nuclei. --- atlas.fit FITS version of atlas table1.tex LaTeX version of Table 1 atlasdoc.tex LaTeX ADC Documentation Nancy Oliversen and Paul Kuin ADC 1995 May 11 UNKNOWN UNKNOWN "An Atlas of Ultraviolet Spectra of Starforming Galaxies" was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Anne Kinney, Space Telescope Science Institute, Baltimore, Maryland. The spectral data for each of the objects were originally contained in 143 separate files. These files were first concatenated into a single file by the data center. The headers for each of the objects were then edited to remove information that was relevant only to the original tape versions of the data (i.e., record and file numbers) and not relevant to the ADC on-line version. Some redundant information was also removed from the headers to make them more readable. The position of fields 6, 7 and 8 (absolute net flux, exposure time, and sigma) varied by 1 byte from object-to-object in the original data files. The information in these three fields were shifted by 1 byte to the right so that all entries were aligned vertically. The affected object numbers were 1, 4, 5, 11-13, 17, 21, 29-30, 32-36, 39-40, 42-44, 48-49, 51-56, 58-59, 61-64, 68-79, 81-86, 88-92, 94-108, 110-114, 116-117, 120-132, 134-135, 140-142. The epsilon and net flux/time fields were edited to align the sign bytes into the same column for each respective field. Table 1 was received from Dr. Anne Kinney in TEX format and was converted to ASCII format by the data center using "dvi2tty" and by realigning the various columns. Documentation within the TEX version of Table 1 (i.e., Notes to Table 1) is included in this ADC document. The galactic longitude of NGC3125 was changed from 365.3 (as it was in the original paper) to 265.3 in the ASCII and TEX versions of Table 1 by the ADC. Cast in ReadMe format May 1995. III_167.xml General Catalog of S Stars, second edition 3168 III/168 General Catalog of S Stars, second edition General Catalog of S Stars, second edition C B Stephenson Publ. Warner & Swasey Observatory 3, no. 1 1 1984 1984gcss.book.....S Stars, late-type Stars, S This catalog is intended to list all Galactic S stars having known positions of at least roughly the precision of the Henry Draper catalog. An S star is a star in whose spectrum the bands of the ZrO molecule are detectable, ordinarily without needing sufficient spectral resolution to resolve the individual rotational lines of a band. In addition, stars exhibiting readily detectable LaO in the photographic infrared, where there is no significant ZrO, are known to form a subset of S stars (more extreme in abundances or low temperature), and this catalog includes stars classified only from the infrared. The majority of the stars were, however, discovered on the basis of the (0,0) band, with head near 6474Angstroem, of the red system of ZrO. Nomenclature Note: There are three catalogues of S stars by Stephenson, each being numbered from 1. Care should therefore be taken to make a clear distinction between a) The first Edition (1976, Publ. Warner & Swasey Obs. 2, No. 2; Catalog <III/60>); these objects are designated "GCSS" b) This second edition published in 1984; these objects are designated "CSS" c) A complement to the Second Edition published in 1990 (=1990AJ....100..569S), designated by "CSS2"
The first edition of this catalog, published more than eight years ago, contained little more than half of the present number of stars, but nearly half of those were previously unpublished although lists of Henize's discoveries had been widely circulated. The principal additions since then come from three sources: (1) A low-dispersion infrared survey of the southern Milky Way by Westerlund, the S stars from which are hitherto unpublished; (2) a relatively high-dispersion red survey by MacConnell, also of the southern Milky Way, published in two lists here catalog-coded as MacCon79 and MacCon82; and (3) an unpublished and just-completed intermediate-dispersion red survey by Stephenson, covering the sky north of declination -25d and outside of galactic latitudes +/-10d. This last survey was intended to create for such red surveys a degree of completeness for the entire sky that was wholly lacking in the first edition. As remarked in the first edition, a logical reason for undertaking this catalog is the author's access to the Observatory's extensive collection of blue, red, and infrared objective prism plates, which covers the entire northern sky (though not in all wavelength regions) plus the southern Milky Way. As before, this collection was used not only for new discoveries, but also to resolve many cases of confusion in the literature. Previous objective prism surveys that were capable of identifying S stars have been summarized by Stephenson in the first edition of this catalog (Stephenson 1976), and also by Yorka and Wing (1979). The best combination of limiting magnitude (mostly 11.5 to 12, visual) and completeness has been achieved in the red spectral region, using the ZrO band with head at 6474 A. The entire northern sky north of declination -25d, plus the southern Milky Way, has been surveyed by Stephenson or N. Sanduleak (who did about 40% of the southern Milky Way), at 1,000 A/mm at H alpha (about 700 A/mm at the D lines). The rest of the southern sky has been done to 10th mag. by K. Henize, using 300 A/mm at the D lines. When the first edition of the S-star catalog was published, there had been no satisfactory red survey (that is, one that was capable of finding S stars consistently) of the sky north of declination -25d and outside of galactic latitudes +/-10d. The author has since remedied this lack, using the Burrell Schmidt telescope. The survey was begun at the old site in Ohio, using improved telescope optics (new corrector plus refigured mirror), but all but some 140 of the nearly 1300 required fields were taken at the Schmidt's new location on Kitt Peak. Also, additional surveys have turned up numbers of S stars in the southern Milky Way. B. Westerlund has used the infrared region at 2100 A/mm to search between galactic latitudes +/-5d and longitudes 235d to 7d, to a limiting infrared magnitude of 12.5. The comparable northern infrared surveys stop about 3 mags. brighter than this, but the author hopes to remedy this situation within a few years. Westerlund's new S stars are published for the first time in the present catalog. MacConnell's new S stars were found with 420 A/mm at H alpha; his plates have the highest spectral resolution of any of the red surveys, and so include the weakest S stars.
The S Star catalog CSS Number The running number in file 1 is newly assigned, but numbers used in the first edition (Catalog <III/60>) are given in the Designations column. --- RAh Right ascension hour (1900) Equatorial coordinates, referred to the equinox and equator which is standard in most spectroscopic tabulations to date, given with varying precision. The coordinates are taken from the various finding lists, and averaged by the author in cases of dual or more determinations of nominally comparable precision. In unresolvable cases of disagreement, the quoted number of significant figures, have been downgraded but the original sources also vary in quoted precision. For many of the objective prism surveys -- including all that have been done at the Warner and Swasey Observatory since 1958 -- the coordinates came from measurements of objective prism plates, using methods described in the Warner and Swasey Observatory Publs. Vol. 2, pp. 74-76. Almost all of the stars for which Stephenson is listed among the designations have independent coordinate determinations from his plates, usually to +/-1" - +/-2". h RAm Right ascension minute (1900) min RAs Right ascension second (1900) s DE- Sign of declination --- DEd Declination degree (1900) deg DEm Declination minute (1900) arcmin DEs Declination second (1900) arcsec bmag b magnitude These are, as available, blue (photographic, sometimes B), visual (sometimes red-biased), and infrared magnitudes. The infrared magnitudes refer generally to the 6800- 8800 A region. For known variable stars, the variable star catalog (GCVS) magnitudes at mid-range are cited under the type of magnitude that was given in the GCVS; other quoted magnitude types for known variables are from survey plates taken at unknown phases. No general statements can be made about the survey-magnitudes at large, and the original papers must be consulted for details. For Stephenson's surveys, blue magnitudes are based upon individually-calibrated plates, and visual ones are based upon an average calibration used for the whole survey; the former may carry +/-0.3 mag. probable error, the latter +/-l mag. In all cases, a value of 0.0 implies no value was available. These values are NOT included in the published catalog, but were tabulated along with the published data. Caveat emptor. mag vmag v magnitude mag imag i magnitude mag GLON Galactic longitude Galactic longitude and latitude, computed by Stephenson. deg GLAT Galactic latitude deg bmag_pub Published b magnitude These magnitude string values are the values published in the Catalog. Some contain the ":" character that indicates that the value given is more uncertain than most. mag vmag_pub Publsihed v magnitude mag imag_pub Published i magnitude mag SpType Spectral type This column furnishes, as available, spectral types in various systems. Omitting sources that are either rare or also used under Designations, the abbreviations define their sources as follows: Bid57 Bidelman (1957) Bid65 Bidelman (1965) CatchF Catchpole & Feast (1971) De Dean (1972) F66 Feast (1966) Houk HD reclassification K Keenan (1954) KB Keenan & Boeshaar (1980) K66 Keenan (1966) K74 Keenan (1974) Merr Merrill (1940) Sanf41 Sanford (1941) Sanf49 Sanford (1949) Sharp Sharpless (1964) WPB Bidelman (1954a) The stars that have been called MS on objective prism plates are in general stronger S stars than those called MS from slit spectrograms, and also -- at least the ones found by Stephenson and colleagues -- are stronger than the weaker S stars published by MacConnell and Henize, who used the highest spectral dispersions of any of the modern surveys. Other spectral symbols may be familiar to most, but will be defined here for completeness: e or E, line emission; p, peculiar; r, uncommonly red; wk or vwk, weak or very weak; S! (used only in Stephenson's surveys), outstanding ZrO strength; colon, uncertainty. Paired numerals flanking either a comma, slash, or asterisk are TiO temperature class and a ZrO strength measure (left to right), in various authors' systems. C-S or SC refer to stars that spectroscopically are nearly intermediate between S-type and carbon stars, due (among other things) to closely comparable abundances of carbon and oxygen. The C-S type was introduced by Stephenson and means stars which in the red spectral region at about 1000 A/mm are very red with strong CN, like an N-type carbon star, but show no definite C2 although they sometimes give the appearance of showing weak-to-moderate 6474 ZrO, which however is uncertain because of the strong CN and low dispersion. In general, given sufficient spectral resolution they can be classified as weak S or weak carbon, although they share many properties of both groups. The SC nomenclature was introduced slightly later and has been used in two ways: to denote all the C-S stars, or alternately those that just fall on the S side, in which convention the carbon S-like group becomes CS. See the discussion in Keenan and Boeshaar (1980). In the present catalog the intent has been to include only the C-S stars that are likely S types. --- Names Designations Here are listed the star's occurrence in various spectroscopic (and some other) finding lists. These are mainly surveys of one kind or another; exceptions will be listed shortly. The author has tried to cite first the earliest survey calling the star an S star (or equivalent, in the case of the HD catalog), Not included here are slit spectrograph observations of known or suspected S stars; those go in the "spectrum" column. Independent spectral classifications are cited here (but not repeated, if already under "spectrum") either if they are quantitative or partially so, or if the star has ever been called a non-S star. The HD number, if one exists, is given without the identifying letters "HD", almost always before anything else. Non-spectroscopic finding list numbers cited are: the HR number, labelled HR; the B.D. or Co.D. numbers, in an obvious notation; and the GCVS (General Catalog of Variable Stars; catalog <II/139>) or CSV (Catalog of Stars Suspected of Being Variable; catalog <II/140>) numbers. CSV numbers are from the editions prior to the 1982 one; they have not been compared with the newest edition of the CSV, partly because of the different equinoxes of that catalog and this one, and partly because it is never particularly noteworthy that an S star has been suspected of variability. Coding of sources: Sources are labelled by the abbreviations given below, with numbers assigned by the corresponding discoverer separated from his abbreviation by a single space. Numbers not separated from the abbreviation are part of the abbreviation, and hyphens if any separate a numbered published table from numbers within the table. The abbreviations mean the following: Bid65 Bidelman (1965). BidK Bidelman and Krumenaker (1972). Bidun Bidelman, unpublished, usually from a slit spectrogram. BidMac Bidelman and MacConnell (1973). BlancN Blanco and Nassau (1957). BM Blanco and Munch (1955). BSD Bergedorfer Spektraldurchmusterung (Schwassmann and Van Rhijn 1935). CatchF Catchpole and Feast (1971). Cra83 Craine et al (1983). D Lee et al (1943, 1944, 1947). The present catalog has not been fully compared with the 44,000 stars of the D lists, except for the stars called S, Sp, or S? De Dean (1972). Dol61 Dolidze (1961). Dol62a " (1962a). Dol62b " (1962b). Dol65 " (1965). Dol68 " (1968). Dol70a " (1970a). Dol70b " (1970b). Dol70c " (1970c). Dol71 " (1971). In most of the lists of this series the coordinates seem to be uncertain by 5' - 10'. Charts for the stars of this series are in Abastumani Bull. Vol. 47, 10, 1975. DolJim Dolidze and Jimsheleishvili (1966). Harw Harwood (1962). Hen60 Henize (1960). Henun Henize, unpublished. These stars are from a list dated 1965, and are in fact published in that they appear in the first edition of the present catalog. Hetzler Hetzler (1937). KB Keenan and Boeshaar (1980). Krum Krumenaker (1975). MacCon MacConnell, unpublished. MacCon67 " (1967). MacCon79 " (1979). MacCon82 " (1982). MacRae MacRae (1952). Merr Merrill (1940). MSB Merrill, Sanford, and Burwell (1933,1942). Without a number, unpublished other than in the first edition of this catalog. Nass54 Nassau, Blanco, and Morgan (1954). NassCam Nassau and Cameron (1956). NassSte Nassau and Stephenson (1961). Without a number, unpublished except for the first ed. of the S-star catalog. Nass64 Nassau, Stephenson and Caprioli (1964). Perr59 Perraud (1959). Perr61 " (1961). Pes Pesch, unpublished (or only in 1st ed. this catalog). Rust Rust (1938). S First edition of this catalog. Sndlk Sanduleak, unpublished (or only in 1st ed. this catalog). Ste Stephenson, " " " " " " " " Ste65 " (1965). Ste73 " (1973). SteTerr Stephenson and Terrill (1967). Sto Stock and Wroblewski (1972). S-WS Two Case lists of S stars: Nassau, Blanco and Morgan (1954); Blanco and Nassau (1957). The68 The (1968). VB Blanco, unpublished except for 1st ed. this catalog. Vys Vyssotsky (1942), Janssen and Vyssotsky (1943), Vyssotsky and Miller (1946), always with a star number. Without a number, Vyssotsky unpublished. VysBalz Vyssotsky and Balz (1958). West'd Westerlund (unpublished). Wray Wray (1966). Numbers are from his combined table of carbon and S stars. His type SE means S with H alpha emission. The various lists occasionally identify with one another, but, except for the BD numbers, most identifications of the stars of one list with those of another have been made by the author. Additional identifications are often given in the Remarks to "notes.dat" file; unlike the first edition, in the present edition the main catalog allots only one line to a given star. If the star was in the first edition of this catalog, its number there is always given here, coded as "S". --- Note Notes Several symbols are used here, as follows. An asterisk means that two or more sources included under "designations" contradict each other as to the star's identity, including cases where a star in an earlier list was published as new in a later list. A single asterisk means that the author's revision of the identification was done without specially examining an objective prism plate, while a double asterisk means the case was specially checked. A plus sign represents a new identification with a GCVS star, done by the author by comparing a plate of the sky with a published identification chart. WPB stands for Bidelman (1954). An R means that there are remarks in the Note to file 1 in notes.dat. References to Case plates in the Notes mean Warner & Swasey Observatory objective prism plates, with the plate examiner almost always being Stephenson Stephenson is always an independent source of uncredited remarks, though not always the earliest such source. --- PosFlag Position accuracy flag The position accuracy is described by the following codes: 1 hh mm ss.s dd mm ss 2 hh mm ss dd mm.m 3 hh mm dd mm --- *Suggested S stars rejected RAa Right ascension (1900) The position accuracy in this file varies. For stars with the higher accuracy, the minutes of right ascension are in bytes 4-5, the seconds of right ascension are in bytes 7-10 and the seconds of declination are in bytes 20-21. For stars whose position accuracy is more crude, the minutes of right ascension are in bytes 7-10 and bytes 20-21 are blank. --- DEa Declination (1900) --- Name Designations --- Note Notes Numerals in parentheses have the following meaning: 1. No candidate star could be found by Stephenson on a blue-region objective prism plate. 2. No candidate star could be found by Stephenson on a red-region objective prism plate. 3. No candidate star could be found by Stephenson on a infrared-region objective prism plate. 4. Candidate star classified by Stephenson on a blue-region objective prism plate. 5. Candidate star classified by Stephenson on a red-region objective prism plate. 6. Candidate star classified by Stephenson on a infrared-region objective prism plate. 7. Slit spectrogram by Stephenson. --- Notes to catalog CSS ? Number --- Note Notes --- refs.txt References reject.txt Notes for reject.dat C. B. Stephenson and N. G. Roman NASA/NSSDC/ADC 1994 May 19 Most of the 1291 fields of my mid-to-high latitude red survey were taken by Warner and Swasey's Kitt Peak resident observer Richard Hill, without whom the survey would have been impossible. For not only the author's own discoveries but also many hundreds of previously-known stars, this catalog incorporates position determinations from Warner and Swasey objective prism plates. Only to mention work done since the first edition, upwards of a dozen undergraduate and graduate students have participated in the measurement and reduction of these plates. The bulk of the appreciable labour of transferring the catalog from file cards to magnetic disk was performed by graduate student Stephen Hulbert. The author is grateful to observers who have communicated unpublished or prepublication discoveries. and for the continued support of the National Science Foundation, without which there would have been no Warner and Swasey surveys and no catalog. III_168.xml IRAS Point Sources of flux at 12 microns greater than flux at 25 microns and falling within about 7 degrees of the Galactic Plane 3170 III/170 IRAS Point Source Identifications IRAS Point Sources of flux at 12 microns greater than flux at 25 microns and falling within about 7 degrees of the Galactic Plane D J MacConnell unpublished, ??? ??? 1993 1993 Infrared sources Stars, late-type The file is an ASCII text file containing the classifications of 14,192 IRAS Point Sources with the flux at 12 microns greater than the flux at 25 microns and falling within about 7 deg of the galactic plane. The aim has been to provide classifications of IRAS PS with no previous associations, so most bright stars such as in the BSC, SAO, and HD which have associations and good spectral types are not included. Also, many known carbon stars from the catalogue of Stephenson known to be associated with PS are not included.
Most of the sources are south of the celestial equator and have been classified in increasing galactic longitude over the period Sept. 1985 to May 1992. They have been classified on Kodak I-N objective-prism plates taken primarily with the Curtis Schmidt telescope at Cerro Tololo, but some northern plates taken with the Burrell Schmidt at Kitt Peak were also used for classification. The spectra cover the range 6800-8800 A at a dispersion of 3400 A/mm at the A-band, and the plate scale is 96.6 "/mm. They are ideal for classifying M stars of type M3 and cooler (increasing strength of TiO and VO bands) and carbon stars (CN bands), but stars warmer than M2 and most S stars cannot be classified or identified as such. The M stars M3 and cooler can be separated into about five groups. The limiting mag of the deepest plates is I about 13.5. The IRAS PS were identified on transparent overlays made to the plate scale for each plate center, and the association of a spectrum with a given PS is usually unambiguous. In cases of doubt or offset, a comment is made. Note that there are some cases where the PSC gives an incorrect association on the basis of position, and the correct association is with a faint, uncatalogued M star.
The catalog of identifications name IRAS Name (Increasing Right Ascension (1950)) --- class Classification --- off Offset from IRAS position arcsec Npl Plate number number=1 l = 60m exposure, sensitized plate m = 30m exposure s = 5m exposure --- NplS Plate number supplement --- den Density on scale of 0 to 20 --- id Identifications / remarks number=2 Not all variable stars, carbon stars, etc. have been identified --- Nancy G. Roman NASA/NSSDC/ADC D. Jack MacConnell STScI 1994 May 02 This work has been supported by the NASA ADP during several cycles, and further funding will be sought to continue classifying beyond the current cut-off in gal. longitude of 314 deg. If there are comments/corrections/ questions, please contact: D. Jack MacConnell macconnell@stsci.edu CSC/STScI Tel.: 410-338-4800 3700 San Martin Drive FAX: 410-338-4767 Baltimore, MD 21218 III_170.xml Radial Velocities from Objective Prism Plates 3172 III/172 Radial Velocities from Objective Prism Plates Radial Velocities from Objective Prism Plates J Stock Rev. Mex. Astron. Astrofis. 24 45 1992 1992RMxAA..24...45S Galactic plane Galactic pole, south Spectral types Radial velocities Accurate positions and radial velocities are determined from 32 objective- prism plates for two areas. Each field is observed twice with opposite dispersion, allowing adjustment of coordinates for spectra not at the plate centers. From the adjusted coordinates and plate overlap, positions are determined with average mean errors: 0.0135 s in RA and 0.177 arcsec in Dec for Area I (near the South Galactic Pole); 0.0315 s in RA, 0.144 arcsec in Dec for Area II (near the galactic plane). Observations were taken by J.D. MacConnell and G. Araya with a six degree prism on the Curtis Schmidt telescope at Cerro Tololo.
Area I (near South Galactic Pole) Area II (near galactic plane, l=270deg) ID Running number --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s e_RAs rms error or right ascension s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec e_DEs rms error or declination arcsec mpg magnitude derived from the density estimates mag RV Radial velocity km/s e_RV rms error on RV km/s Sp spectral type --- Np Number of plates --- J.A.W. SSDOO/ADC 1996 Aug 12 CDS thanks Dr Jurgen Stock for having kindly mailed the data in electronic form. UNKNOWN UNKNOWN 20-Jul-1993 F. Ochsenbein [CDS] original III_172.xml An Atlas of High Resolution Line Profiles of Symbiotic Stars wIII/174 wIII/174 High Resolution Atlas of Symbiotic Stars An Atlas of High Resolution Line Profiles of Symbiotic Stars H Van Winckel H W Duerbeck H E Schwarz Astron. Astrophys. Suppl. Ser. 102 401 1993 1993A&AS..102..401V An Atlas of High Resolution Line Profiles of Symbiotic Stars R J Ivison M F Bode J Meaburn Astron. Astrophys. Suppl. Ser. 103 201 1994 1994A&AS..103..201I Atlases Novae Stars, double and multiple This catalog contains a high resolution atlas of both northern and southern sky symbiotic stars. It represents an all-sky optical survey of symbiotic stars using Echelle spectrometers. A summary of the stars with positions and a summary of spectra available are included. The wavelength resolution is better than 0.01 nm. The emission lines in this catalog were chosen to allow the determination of global values for the density and temperature of the nebula, as well as the temperature of the ionizing source. Note that some of the spectra with date marked by "+++" in the "Date" column of the "spectra.dat" file are not in the original publications.
List of Symbiotic stars in this catalog File File name Catalog file numbered starting with s001 to s059 are from van Winckel et al, A&AS 102, 401; those with numbers s101 to s135 are from Ivison et al., A&AS 103, 201. Stars common to both publications have been merged. These are: s024 = s107 = T CrB s030 = s110 = RT Ser s033 = s111 = RS Oph s037 = s112 = H 2-38 s038 = s113 = AS 289 s041 = s115 = AS 296 s053 = s119 = CM Aql s056 = s128 = PU Vul s058 = s133 = AG Peg s059 = s135 = R Aqr s105 = s006 = BX Mon s118 = s052 = V919 Sgr Subsequent spectra of the stars have been extracted into files with the same filestem followed by an underscore and a number. --- S/D-type Star or Dust type --- Name Star name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Lin 358 Ha 13-12-88 Lin 358 Ha 18-10-88 Lin 358 HeII 19-10-88 Lin 358 OIII 15-12-88 Lin 358 Ha 19-07-88 Lin 358 HeI 20-10-88 Lin 358 HeII 23-07-88 Lin 358 OIII 21-10-88 Lin 358 SII 18-10-88 N 73 Ha 13-12-88 MA 1858 Ha 14-12-88 Sanduleak's st Ha 13-12-88 S63 Ha 13-12-88 S63 HeI 13-12-88 S63 OIII 15-12-88 BX Mon Ha 14-12-88 BX Mon LR +++1987 BX Mon HeI 20-10-88 BX Mon OIII 21-10-88 BX Mon Ha 06-05-90 Wray 157 Ha 14-12-88 Wray 157 HeI 13-12-88 Wray 157 HeII 19-10-88 Wray 157 OIII 15-12-88 RX Pup OIII 14-12-88 RX Pup Ha 15-12-88 RX Pup HeI 20-10-88 RX Pup OIII 21-10-88 He3-160 Ha 14-12-88 He3-160 HeI 13-12-88 He3-160 OIII 15-12-88 AS 201 Ha 14-12-88 AS 201 HeI 12-12-88 AS 201 OIII 22-10-88 He2-38 Ha 18-07-88 He2-38 HeI 20-07-88 He2-38 HeII 21-07-88 He2-38 OIII 15-12-88 He2-38 SII 24-07-88 SY Mus Ha 14-07-88 SY Mus HeI 20-07-88 SY Mus HeII 23-07-88 SY Mus OIII 16-07-88 BI Cru Ha 15-07-88 BI Cru HeI 20-07-88 BI Cru HeII 23-07-88 BI Cru OIII 18-07-88 He3-828 Ha 19-07-88 He3-863 Ha 15-07-88 He3-863 HeI 20-07-88 He3-863 OIII 18-07-88 St2-22 Ha 12-07-92 St2-22 Ha 19-07-88 He3-886 Ha 14-07-88 He3-886 HeI 21-07-88 He3-886 HeII 22-07-88 He3-886 OIII 18-07-88 RW Hya Ha 10-07-92 RW Hya Ha 13-07-88 RW Hya HeI 20-07-88 RW Hya HeII 23-07-88 RW Hya OIII 16-07-88 He2-104 Ha 19-07-88 He2-104 HeI 21-07-88 He2-104 HeII 22-07-88 He2-104 OIII 18-07-88 He2-104 SII 24-07-88 He2-106 Ha 19-07-88 He2-106 HeI 21-07-88 He2-106 SII 24-07-88 V417 Cen Ha 19-07-88 V417 Cen OIII 18-07-88 BD-21 3873 Ha 14-07-88 BD-21 3873 HeI 21-07-88 BD-21 3873 HeII 22-07-88 BD-21 3873 OIII 17-07-88 HD 330036 Ha 15-07-88 HD 330036 HeI 21-07-88 HD 330036 OIII 16-07-88 He2-171 Ha 19-07-88 He2-171 SII 24-07-88 He3-1213 Ha 11-07-92 He3-1213 HeI 20-07-88 He3-1213 HeII 23-07-88 KX TrA Ha 15-09-89 KX TrA OIII 18-09-89 CL Sco Ha 15-09-89 CL Sco OIII 18-09-89 He3-1341 Ha 15-09-89 AE Ara Ha 14-07-88 AE Ara HeI 20-07-88 AE Ara HeII 23-07-88 AE Ara OIII 16-07-88 H1-36 Ha 15-09-89 H1-36 OIII 17-09-89 V745 Sco Ha 16-07-92 AS 255 Ha 10-09-89 AS 270 Ha 15-09-89 Y CrA Ha 14-07-88 Y CrA HeI 20-07-88 Y CrA HeII 23-07-88 Y CrA OIII 16-07-88 Y CrA SII 24-07-88 HD 319167 Ha 09-09-89 AR Pav Ha 14-07-88 AR Pav HeI 21-07-88 AR Pav HeII 22-07-88 AR Pav OIII 16-07-88 AR Pav SII 26-09-88 He2-390 Ha 19-07-88 He2-390 HeI 21-07-88 V3804 Sgr Ha 09-09-89 V3804 Sgr OIII 18-09-89 AS 304 Ha 14-09-89 AS 304 OIII 12-07-92 V3890 Sgr Ha 16-07-92 V1017 Sgr Ha 16-09-89 AS 316 Ha 16-09-89 MWC 960 Ha 09-09-89 MWC 960 OIII 17-09-89 AS 327 Ha 19-07-88 AS 327 HeI 21-07-88 AS 327 HeII 22-07-88 AS 327 OIII 12-07-92 FN Sgr Ha 10-09-89 FN Sgr Ha 15-07-88 FN Sgr HeI 21-07-88 FN Sgr HeII 22-07-88 FN Sgr OIII 17-07-88 FN Sgr SII 26-09-88 V919 Sgr Ha 10-09-89 V919 Sgr HeII 20-10-88 V919 Sgr Ha 15-07-88 V919 Sgr HeI 21-07-88 V919 Sgr HeII 22-07-88 V919 Sgr OIII 17-07-88 V919 Sgr HeII 31-07-91 V919 Sgr OIII 01-08-91 V919 Sgr Ha 01-08-91 He3-1761 Ha 15-07-88 He3-1761 HeI 20-07-88 He3-1761 HeII 17-07-88 He3-1761 OIII 16-07-88 He3-1761 SII 24-07-88 He3-1761 Ha 18-10-88 He3-1761 HeI 19-10-88 He3-1761 HeII 20-10-88 He3-1761 OIII 17-09-89 RR Tel Ha 14-07-88 RR Tel HeI 15-07-88 RR Tel HeII 17-07-88 RR Tel OIII 16-07-88 RR Tel SII 24-07-88 CD-43 14304 Ha 14-07-88 CD-43 14304 HeI 19-10-88 CD-43 14304 HeII 23-07-88 CD-43 14304 OIII 16-07-88 CD-43 14304 SII 24-07-88 CD-43 14304 Ha 18-10-88 CD-43 14304 HeII 20-10-88 EG And HeII 21-09-88 EG And OIII 21-09-88 EG And LR 26-09-88 EG And Ha 21-09-88 EG And LR +++1989 AX Per HeII 22-09-88 AX Per HeII 20-09-89 AX Per HeII 01-08-91 AX Per OIII 22-09-88 AX Per OIII 19-09-89 AX Per OIII 01-08-91 AX Per LR 26-09-88 AX Per LR 30-07-91 AX Per Ha 22-09-88 AX Per Ha 19-09-89 AX Per Ha 01-08-91 AX Per Ha +++1990 AX Per HeII +++1990 AX Per OIII +++1990 AX Per LR +++1989 V741 Per HeII 21-09-88 V741 Per HeII 31-07-91 V741 Per OIII 21-09-88 V741 Per OIII 29-07-91 V741 Per LR 26-09-88 V741 Per LR 17-09-89 V741 Per LR 30-07-91 V741 Per Ha 21-09-88 V741 Per Ha 29-07-91 UV Aur HeII 23-09-88 UV Aur OIII 23-09-88 UV Aur LR 26-09-88 UV Aur Ha 23-09-88 TX CVn HeII 20-06-89 TX CVn OIII 19-06-89 TX CVn Ha 19-06-89 TX CVn Ha 04-05-90 TX CVn LR +++1990 T CrB Ha 14-07-88 T CrB HeII 22-07-88 T CrB OIII 17-07-88 T CrB HeII 20-06-89 T CrB OIII 20-06-89 T CrB OIII 04-05-90 T CrB Ha 19-06-89 T CrB Ha 03-05-90 T CrB LR +++1990 AG Dra Ha 18-06-86 AG Dra Ha 20-06-89 AG Dra HeII 20-06-89 AG Dra OIII 20-06-89 AG Dra Ha 04-05-90 AG Dra LR +++1990 AS 210 HeII 30-07-91 AS 210 OIII 30-07-91 AS 210 Ha 30-07-91 RT Ser Ha 15-07-88 RT Ser HeII 23-07-88 RT Ser OIII 18-07-88 RT Ser HeII 28-07-91 RT Ser OIII 28-07-91 RT Ser LR 29-07-91 RT Ser Ha 28-07-91 RT Ser LR +++1986 RS Oph Ha 10-09-89 RS Oph Ha 15-07-88 RS Oph HeI 20-07-88 RS Oph HeII 23-07-88 RS Oph OIII 16-07-88 RS Oph Ha 15-07-92 RS Oph LR 07-05-90 RS Oph Ha 28-06-86 RS Oph Ha 06-07-87 RS Oph Ha 06-05-90 RS Oph Ha 27-07-91 RS Oph LR +++1986 H 2-38 Ha 16-09-89 H 2-38 OIII 18-09-89 H 2-38 HeII 30-07-91 H 2-38 OIII 01-08-91 H 2-38 LR 29-07-91 H 2-38 Ha 01-08-91 AS 289 Ha 15-09-89 AS 289 Ha 06-05-90 AS 289 LR 07-05-90 AS 289 Ha 17-09-89 AS 289 HeII 17-09-89 AS 289 LR 16-09-89 AS 289 OIII 17-09-89 YY Her HeII 20-06-89 YY Her OIII 20-06-89 s114_3.dat 20 0 YY Her LR 23-06-89 </tableLink> <tableLink xlink:href="s114_4.dat"> <title>YY Her Ha 20-06-89 AS 296 Ha 16-09-89 AS 296 HeII 22-07-88 AS 296 HeII 28-07-91 AS 296 OIII 27-07-91 AS 296 LR 29-07-91 AS 296 Ha 27-07-91 V443 Her HeII 20-06-89 V443 Her HeII 04-05-90 V443 Her OIII 20-06-89 V443 Her LR 07-05-90 V443 Her Ha 20-06-89 V443 Her Ha 04-05-90 Pe 2-16 HeII 17-09-89 Pe 2-16 LR 16-09-89 Pe 2-16 Ha 17-09-89 CM Aql Ha 09-09-89 CM Aql HeII 18-09-89 CM Aql OIII 18-09-89 CM Aql LR 16-09-89 CM Aql Ha 18-09-89 AS 338 HeII 22-06-89 AS 338 HeII 19-09-89 AS 338 OIII 19-09-89 s120_4.dat 20 0 AS 338 LR 23-06-89 </tableLink> <tableLink xlink:href="s120_5.dat"> <title>AS 338 LR 16-09-89 AS 338 LR 07-05-90 AS 338 Ha 22-06-89 AS 338 Ha 18-09-89 Ap 3-1 HeII 19-09-89 Ap 3-1 LR 16-09-89 Ap 3-1 Ha 19-09-89 BF Cyg HeII 21-09-88 BF Cyg OIII 21-09-88 BF Cyg OIII 06-05-90 BF Cyg LR 25-09-88 BF Cyg LR 07-05-90 BF Cyg Ha 21-09-88 BF Cyg Ha 06-05-90 CH Cyg Ha 18-06-86 CH Cyg Ha 07-07-87 CH Cyg Ha +++1988 CH Cyg Ha 20-09-88 CH Cyg Ha 19-06-89 CH Cyg Ha 15-09-89 CH Cyg Ha 03-05-90 CH Cyg Ha 23-07-91 CH Cyg OIII +++1988 CH Cyg OIII 28-06-86 CH Cyg OIII +++1987 CH Cyg OIII +++1988 CH Cyg OIII 03-05-90 CH Cyg OIII 19-06-89 CH Cyg OIII 23-07-91 CH Cyg HeII 23-07-91 CH Cyg LR 30-07-91 CH Cyg LR 07-05-90 CH Cyg LR 25-09-88 CH Cyg OIII 20-09-88 CH Cyg LR 17-09-89 CH Cyg OIII 15-09-89 HM Sge HeII 23-09-88 HM Sge HeII 16-09-89 HM Sge HeII 05-05-90 HM Sge HeII 28-07-91 HM Sge OIII 28-06-86 HM Sge OIII 23-09-88 HM Sge OIII 16-09-89 HM Sge OIII 05-05-90 HM Sge OIII 28-07-91 HM Sge LR 25-09-88 HM Sge LR 17-09-89 HM Sge LR 07-05-90 HM Sge LR 30-07-91 HM Sge Ha 30-06-86 HM Sge Ha 23-09-88 HM Sge Ha 16-09-89 HM Sge Ha 05-05-90 HM Sge Ha 28-07-91 AS 360 Ha 06-05-90 AS 360 HeII 06-05-90 AS 360 Ha 23-09-88 AS 360 HeII 23-09-88 AS 360 LR +++1988 AS 360 OIII 23-09-88 CI Cyg HeII 21-09-88 CI Cyg HeII 16-09-89 CI Cyg OIII 21-09-88 CI Cyg OIII 20-06-89 CI Cyg OIII 16-09-89 CI Cyg LR 17-09-89 CI Cyg LR 07-05-90 CI Cyg Ha 21-09-88 CI Cyg Ha 20-06-89 CI Cyg Ha 16-09-89 CI Cyg Ha 04-05-90 CI Cyg LR +++1988 V1016Cyg HeII 22-09-88 V1016Cyg HeII 19-09-89 V1016Cyg HeII 06-05-90 V1016Cyg OIII 28-06-86 V1016Cyg OIII 22-09-88 V1016Cyg OIII 16-09-89 V1016Cyg OIII 06-05-90 V1016Cyg LR 17-09-89 V1016Cyg LR 30-07-91 V1016Cyg Ha 30-06-86 V1016Cyg Ha 22-09-88 V1016Cyg Ha 16-09-89 V1016Cyg Ha 07-05-90 V1016Cyg Ha 02-08-91 V1016Cyg LR +++1990 PU Vul LR 07-05-90 PU Vul Ha 06-05-90 PU Vul Ha 15-09-89 PU Vul Ha 28-09-88 PU Vul OIII 29-09-88 PU Vul OIII +++1986 PU Vul LR +++1989 He 2-467 HeII 22-09-88 He 2-467 OIII 22-09-88 He 2-467 Ha 22-09-88 He 2-467 LR +++1989 He 2-468 HeII 22-09-88 He 2-468 HeII 31-07-91 He 2-468 OIII 22-09-88 He 2-468 OIII 31-07-91 He 2-468 Ha 22-09-88 He 2-468 Ha 31-07-91 He 2-468 LR +++1989 V1329Cyg HeII 21-09-88 V1329Cyg HeII 16-09-89 V1329Cyg HeII 29-07-91 V1329Cyg OIII 28-06-86 V1329Cyg OIII 21-09-88 V1329Cyg OIII 20-09-89 V1329Cyg OIII 29-07-91 V1329Cyg LR 26-09-88 V1329Cyg LR 17-09-89 V1329Cyg LR 30-07-91 V1329Cyg Ha 30-06-86 V1329Cyg Ha 21-09-88 V1329Cyg Ha 16-09-89 V1329Cyg Ha 06-05-90 V1329Cyg Ha 29-07-91 V407 Cyg OIII 23-09-88 V407 Cyg LR 30-07-91 V407 Cyg Ha 23-09-88 V407 Cyg Ha 02-08-91 V407 Cyg LR +++1988 AG Peg Ha 15-07-88 AG Peg HeI 21-07-88 AG Peg HeII 22-07-88 AG Peg OIII 17-07-88 AG Peg SII 26-09-88 AG Peg HeII 21-09-88 AG Peg HeII 19-09-89 AG Peg HeII 29-07-91 AG Peg OIII 20-09-88 AG Peg OIII 19-09-89 AG Peg OIII 29-07-91 AG Peg LR 17-09-89 AG Peg LR 30-07-91 AG Peg Ha 30-06-86 AG Peg Ha 07-07-87 AG Peg Ha 20-09-88 AG Peg Ha 19-09-89 AG Peg Ha 29-07-91 AG Peg Ha +++1989 AG Peg LR +++1990 Z And HeII 22-09-88 Z And OIII 22-09-88 Z And LR 26-09-88 Z And Ha 30-06-86 Z And Ha 07-07-87 Z And Ha 22-09-88 R Aqr Ha 14-07-88 R Aqr HeII 17-07-88 R Aqr OIII 16-07-88 R Aqr SII 24-07-88 R Aqr Ha 18-10-88 R Aqr HeII 19-10-89 R Aqr OIII 29-07-91 R Aqr LR 30-07-91 R Aqr Ha 30-06-86 R Aqr Ha 29-07-91 wavel wavelength 0.1nm flux flux in 10**-15 W cm**-2 micron**-1 10-11W/m2/um Summary of spectra Star name Sp.region date File File name --- Date Date of the observation (DD-MM-YY format) --- SpecR Region of the spectrum Wavelength region in terms of spectral feature, e.g., Ha = Halpha, HeI = neutral Helium, etc. (LR = Low Resolution Spectrum) --- Points Number of points in the spectrum --- F. Ochsenbein CDS C.-H. J. Lyu, P. Kuin NASA/ADC 1996 Oct 18 There was no previous ADC documentation. The original publications (van Winckel et al. 1993; Ivison et al. 1994) were used to create this ReadMe file (Lyu, ADC, 1996). The original data were merged spectra per star. The individual spectra were each put in one file to allow for automated handling and access (Kuin, ADC, 1996). The FITS version was created using a CDS script on the original files (Ochsenbein, CDS). wIII_174.xml Optical spectroscopy of 1Jy, S4 and S5 radio source identifications 3175 III/175 Optical spectroscopy of radio sources Optical spectroscopy of 1Jy, S4 and S5 radio source identifications M Stickel H Kuehr J W Fried Astron. Astrophys. Suppl. Ser. 80 103 1989 1989A&AS...80..103S Optical spectroscopy of 1Jy, S4 and S5 radio source identifications M Stickel H Kuehr J W Fried Astron. Astrophys. Suppl. Ser. 97 483 1993 1993A&AS...97..483S Optical spectroscopy of 1Jy, S4 and S5 radio source identifications M Stickel H Kuehr J W Fried Astron. Astrophys. Suppl. Ser. 100 395 1993 1993A&AS..100..395S Optical spectroscopy of 1Jy, S4 and S5 radio source identifications M Stickel H Kuehr J W Fried Astron. Astrophys. Suppl. Ser. 101 521 1993 1993A&AS..101..521S Optical spectroscopy of 1Jy, S4 and S5 radio source identifications M Stickel H Kuehr J W Fried Astron. Astrophys. Suppl. Ser. 103 349 1994 1994A&AS..103..349S J/A+AS/98/393 : (II-Observational data) J/A+AS/105/67 : (Optical identifications from 1Jy, S4, S5) J/A+AS/105/211 : (Optical identification of 1Jy) J/A+AS/115/1 : (Optical identifications from S5 catalog) J/A+AS/115/11 : (Optical identifications from 1Jy, S4, S5) Radio sources Active gal. nuclei QSOs Redshifts galaxies: active quasars: emission lines radio continuum: galaxies radio continuum: general An update of the optical identification status of the S4 radio source catalogue is presented. An extensive literature search has been made to gather the types of the optical counterparts, their magnitudes and redshifts. As far as possible, references to other optical catalogues are given for these data, which are often supplemented by more detailed notes on individual sources. Accurate radio positions taken from the literature are given for a large fraction of the sources.
Observed radio source identifications Object Object name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec m Magnitude of the optical identification mag Type Type of the optical identification --- S5GHz 5GHz flux Jy s(11-6) Two-point spectral index between 11 and 6 cm --- Names Entries in other radio sources catalogues --- Journal of the observations Object Object name --- Tel Telescope number=1 Telescopes: CA 3.5 = 3.5 m telescope on Calar Alto, Spain CA 2.2 = 2.2 m telescope on Calar Alto, Spain LS 2.2 = 2.2 m telescope on La Silla, Chile --- Date Observation date --- IntTime Total integration time s Scale Scale of the wavelength calibrated spectra. 0.1nm/pix Scale2 Scale in in red channel for Twin Spectrograph 0.1nm/pix Line data Object Object name --- l_z ">" sign for lower redshift limit --- z Redshift computed from unweighted zInd --- Element Element identification --- Lam0 Rest wavelength 0.1nm u_Lam0 ? when unknown --- LamObs Observed wavelength 0.1nm zInd Individual redshift --- u_zInd ? when unknown --- FWHM FWHM (for emission line) 0.1nm EW Equivalent width (for emission line) 0.1nm u_EW ":" sign indicating uncertain values --- Flux Flux (10-16erg/s/cm2) 10-19W/m2 u_Flux ":" sign indicating uncertain values --- Rem Remarks number=1 gal = stellar absorption lines of host galaxy abs = intervening absorption lines cal = calibration uncertain due to second order contamination atm = emission lines affected by atmospheric absorption --- Patricia Bauer CDS 1994 Nov 25 Manfred Stickel <stickel@mpia-hd.mpg.de> III_175.xml Survey Observations of Emission-line Stars in the Orion Region I. The Kiso Area A-0904 3177 III/177 H-alpha emission stars in the Orion region Survey Observations of Emission-line Stars in the Orion Region I. The Kiso Area A-0904 S D Wiramihardja T Kogure S Yoshida K Ogura M Nakano Publ. Astron. Soc. Japan 41 155 1989 1989PASJ...41..155W Survey Observations of Emission-line Stars in the Orion Region I. The Kiso Area A-0904 T Kogure S Yoshida S D Wiramihardja M Nakano T Iwata K Ogura Publ. Astron. Soc. Japan 41 1195 1989 1989PASJ...41.1195K Survey Observations of Emission-line Stars in the Orion Region I. The Kiso Area A-0904 S D Wiramihardja T Kogure S Yoshida M Nakano K Ogura T Iwata Publ. Astron. Soc. Japan 43 27 1991 1991PASJ...43...27W Survey Observations of Emission-line Stars in the Orion Region I. The Kiso Area A-0904 S D Wiramihardja T Kogure K Ogura S Yoshida M Nakano Publ. Astron. Soc. Japan 45 643 1993 1993PASJ...45..643W Stars, emission Extensive survey observations were carried out for H-alpha emission stars in six Kiso Areas in the Orion region. The observations were made using mainly the Kiso Schmidt telescope, and partly using the CTIO Curtis Schmidt telescope. Our surveys extends the limiting magnitude to V=17.5 over an area of 150 square degrees, and the total number of detected H-alpha emission stars were 1157. The celestial coordinates and the V magnitudes were measured along with an eye estimation of the H-alpha intensities. The identification from the previous observations were also made. The brightness distribution, which is peaked around V=15, suggests that they are probable candidates of T Tauri-type stars.
H-alpha emission-line stars in Ori region area Area number number=1 The 6 area numbers are as follows: ----------------------------------------------- Kiso Area central position paper R.A. Dec. ---------------------------------------------- 03 A0903 5:20 0:00 II 04 A0904 5:40 0:00 I 75 A0975 5:20 - 5:00 III 76 A0976 5:40 - 5:00 III 47 A1047 5:20 -10:00 IV 48 A1048 5:40 -10:00 IV --- seq Serial number in each area in increasing R.A. order at epoch of 1950.0. --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec INT1 Estimated H-alpha emission intensity number=2 For A0904 and A0976, at three and two epochs of observations, respectively. The scale of emission intensity is given by the six grades of 5 (very strong), 4 (strong), 3 (medium), 2 (weak), 1 (very weak), 0 (absent or doubtful), and 9 means that it lies out of area on the CTIO plates. --- INT2 Second estimated H-alpha emission intensity --- INT3 Third estimated H-alpha emission intensity --- Vmag V magnitude number=3 "99.9" indicates unreliable magnitude measurement by several causes, such as unseparated double star image, saturated bright star image, contamination by nebulosities. "=>" indicates another number of the same object appearing in this catalogue beforehand; a "*" indicates a note in file notes.dat (4) mag Notes Identification with the previous surveys number=4 "=>" indicates another number of the same object appearing in this catalogue beforehand "*" indicates a note in file notes.dat Abbreviations used for the headings in the respective current ID numbers are given below: -------------------------------------------------------------------------- B Bernes, =1977A&AS...29...65B Brun Brun, =1935POLyo...1...12B H Haro, =1953ApJ...117...73H HM Haro & Moreno(1953) Bol.Obs.Tonantzintla Tacubaya 7,11. =1953BOTT....1g..11H HBC Herbig & Bell (1988) Lick Obs. Bulletin No.111. =1988LicOB1111....1H; Catalog <V/73> HK Herbig & Kuhi =1963ApJ...137..398H IRAS IRAS Point Source Catalog, Catalog <II/125> L LkHa-number (Herbig & Kuhi =1963ApJ...137..398H; Herbig & Rao 1972ApJ...174..401H). M78/ Strom et al. =1975ApJ...196..489S NK Nakajima et al. =1986MNRAS.221..483N NGC2068 Sellgren =1983AJ.....88..985S OH Ogura & Hasegawa =1983PASJ...35..299O P Parenago (1954) Trudy Sternberg Astr. Inst. 25,1. =1954TrSht..25....1P ; Catalog <II/171> PC Parsamyan & Chavira (1982) Bol.del Inst. de Tonantzintla 3,69. San Sanduleak =1971PASP...83...95S SSV Strom et al. =1976AJ.....81..308S St Stephenson =1986ApJ...300..779S STR Strom et al. =1989ApJS...71..183S Ton rapid variables found by Haro & Morgan =1953ApJ...118...16H; Haro (1954) Bol Ton y Tac 2, nr 11, 11., and Haro & Rivera Terrazas (1954) Bol Ton y Tac 1, nr 10, 3. V Variable stars. X Strom et al. =1990ApJ...362..168S -------------------------------------------------------------------------- -------------------------------------------------------------------------------- Byte-by-byte Description of file: notes.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 I2 --- area Area number, as in catalog 3- 5 I3 --- seq Serial number, as in catalog 8- 58 A51 --- Text Text of note --- S.Nishimura, K.Nakajima ADAC/NAOJ 1994 Aug 11 UNKNOWN UNKNOWN * 11-Aug-1994: The machine-readable version of this catalogue was compiled by M. Nakano at Oita University, and reformatted and documented at the Astronomical Data Analysis Center, the National Astronomical Observatory of Japan. * 24-Feb-1998: the notes have been gathered into the notes.dat file. (F. Ochsenbein, CDS) III_177.xml An Atlas of Southern MK Standards from 5800 to 10,200 Angstroms 3179 III/179 Southern MK Standards 5800-10200A An Atlas of Southern MK Standards from 5800 to 10,200 Angstroms A C Danks M Dennefeld Pub. Astron. Soc. Pac. 106 382 1994 1994PASP..106..382D Stars, standard Spectra, red Spectra are presented for 126 MK standards in the wavelength range 5800 to 10200 A. The stars cover the normal spectral types O to M and luminosity types I, III, and V. In addition, a small number of peculiar stars are included. The data are in 137 FITS files.
The projected slit width along the dispersion was about 4 A, slightly less than 2 pixels. The data are corrected for atmospheric extinction. The fluxes are relative. To convert to "absolute" the values should be multiplied by 10**-13 ergs/sq. cm/s/A but because not all of the flux was collected by the slit, these values will be about 15% low with the factor depending on the seeing. Some features in the spectrum have been introduced by the instrumentation. The most notable feature is a small emission peak near the Na I 5896 A absorption line. The data are in FITS format. The FITS header does not include the units, which are described above. The spectral types and luminosity classes given in the published paper supersede those given in the FITS headers.
HD66811.fit spectrum of HD 66811 O5F HD37742.fit spectrum of HD 37742 O9I HD57061.fit spectrum of HD 57061 O9I HD37043.fit spectrum of HD 37043 O9 III HD47839.fit spectrum of HD 47839 O7V HD37468.fit spectrum of HD 37468 09V HD38771.fit spectrum of HD 38771 B0.5I HD53138.fit spectrum of HD 53138 B3IA HD58350.fit spectrum of HD 58350 B5IA HD164353.fit spectrum of HD 164353 B5IB HD34085.fit spectrum of HD 34085 B8I HD44743.fit spectrum of HD 44743 B1II HD51309.fit spectrum of HD 51309 B3II HD53244.fit spectrum of HD 53244 B8II HD30836.fit spectrum of HD 30836 B2III HD35468.fit spectrum of HD 35468 B2 III HD34503.fit spectrum of HD 34503 B4III HD147165.fit spectrum of HD 147165 B1IV HD143018.fit spectrum of HD 143018 B2IV HD16582.fit spectrum of HD 16582 B2IV HD23302.fit spectrum of HD 23302 B6IV HD23630.fit spectrum of HD 23630 B7IV HD23850.fit spectrum of HD 23850 B8IV HD35411.fit spectrum of HD 35411 B1V HD149438.fit spectrum of HD 149438 B0V HD144470.fit spectrum of HD 144470 B1V HD74280.fit spectrum of HD 74280 B2V HD208057.fit spectrum of HD 208057 B3V HD219688.fit spectrum of HD 219688 B5V HD214923.fit spectrum of HD 214923 B8V HD218045.fit spectrum of HD 218045 B9V HD46300.fit spectrum of HD 46300 AOIB HD59612.fit spectrum of HD 59612 A5IB HD43836.fit spectrum of HD 43836 B9II HD47306.fit spectrum of HD 47306 A2II HD73634.fit spectrum of HD 73634 A9II HD216627.fit spectrum of HD 216627 A2III HD33111.fit spectrum of HD 33111 A3III HD28319.fit spectrum of HD 28319 A7III HD48843.fit spectrum of HD 48843 FO HD47105.fit spectrum of HD 47105 A0IV HD161868.fit spectrum of HD 161868 A0V HD71155.fit spectrum of HD 71155 AOV HD198001.fit spectrum of HD 198001 A1V HD18331.fit spectrum of HD 18331 A1V HD222095.fit spectrum of HD 222095 GO HD155125.fit spectrum of HD 155125 A2V HD55179.fit spectrum of HD 55179 A2 HD11636.fit spectrum of HD 11636 A5V HD187642.fit spectrum of HD 187642 A7V HD88824.fit spectrum of HD 88824 A5 HD36673.fit spectrum of HD 36673 F0IB HD90772.fit spectrum of HD 90772 F0I HD161471.fit spectrum of HD 161471 F2IA HD61715.fit spectrum of HD 61715 F4 HD54605.fit spectrum of HD 54605 F8I HD38558.fit spectrum of HD 38558 FOIII HD13174.fit spectrum of HD 13174 F2III HD164584.fit spectrum of HD 164584 F3III HD27290.fit spectrum of HD 27290 HD48737.fit spectrum of HD 48737 F4I HD196524.fit spectrum of HD 196524 F5III HD217096.fit spectrum of HD 217096 F8III HD220657.fit spectrum of HD 220657 F8III HD17094.fit spectrum of HD 17094 FOIV HD27397.fit spectrum of HD 27397 F0IV HD182640.fit spectrum of HD 182640 F3 HD216385.fit spectrum of HD 216385 F7IV HD29992.fit spectrum of HD 29992 F2 HD26690.fit spectrum of HD 26690 F3V HD30652.fit spectrum of HD 30652 F6V HD173667.fit spectrum of HD 173667 F6V HD222368.fit spectrum of HD 222368 F7V HD1581.fit spectrum of HD 1581 G0 HD204867.fit spectrum of HD 204867 G0IB HD52220.fit spectrum of HD 52220 G1 HD209750.fit spectrum of HD 209750 G2IB HD44362.fit spectrum of HD 44362 G2I HD206859.fit spectrum of HD 206859 G5IB HD48329.fit spectrum of HD 48329 G8I HD36079.fit spectrum of HD 36079 G5II HD185758.fit spectrum of HD 185758 G1III HD21120.fit spectrum of HD 21120 G6III HD33833.fit spectrum of HD 33833 G7 HD10761.fit spectrum of HD 10761 G8III HD184492.fit spectrum of HD 184492 G9III HD195564.fit spectrum of HD 195564 G2IV HD188512.fit spectrum of HD 188512 G8 HD39587.fit spectrum of HD 39587 G0V HD214850.fit spectrum of HD 214850 G3V HD20630.fit spectrum of HD 20630 G5 HD69830.fit spectrum of HD 69830 G7V HD206778.fit spectrum of HD 206778 K2IB HD185622.fit spectrum of HD 185622 K4IB HD179870.fit spectrum of HD 179870 K0II HD31767.fit spectrum of HD 31767 K2II HD167818.fit spectrum of HD 167818 K3II HD8512.fit spectrum of HD 8512 KOIII HD39810.fit spectrum of HD 39810 KOI HD211416.fit spectrum of HD 211416 K3III HD23719.fit spectrum of HD 223719 K4III HD23249.fit spectrum of HD 23249 K0IV HD3651.fit spectrum of HD 3651 K0V HD22049.fit spectrum of HD 22049 K2V HD36389.fit spectrum of HD 36389 M2I HD200914.fit spectrum of HD 200914 M0.5II HD216032.fit spectrum of HD 216032 M0+III HD219215.fit spectrum of HD 219215 M1.5II HD198026.fit spectrum of HD 198026 M3III HD19285.fit spectrum of HD 19285 M5III HD184313.fit spectrum of HD 184313 M5III HD207076.fit spectrum of HD 207076 M7III HD202560.fit spectrum of HD 202560 M0 HD36395.fit spectrum of HD 36395 M1.5V HD217987.fit spectrum of HD 217987 M3 HD180617.fit spectrum of HD 180617 M3V HD49798.fit spectrum of HD 49798 OE 5 HD37490.fit spectrum of HD 37490 B3 P HD49333.fit spectrum of HD 49333 B8 HD5737.fit spectrum of HD 5737 B5 HD315.fit spectrum of HD 315 A0M HD12767.fit spectrum of HD 12767 AP HD92207.fit spectrum of HD 92207 A0IE HD62623.fit spectrum of HD 62623 HD18557.fit spectrum of HD 18557 HD20320.fit spectrum of HD 20320 AM HD67523.fit spectrum of HD 67523 F6IIP HD189005.fit spectrum of HD 189005 G6III HD223541.fit spectrum of HD 223541 K0III HD223428.fit spectrum of HD 223428 K2III HD1157.fit spectrum of HD 1157 K0 HD170975.fit spectrum of HD 170975 K3III HD46259.fit spectrum of HD 46259 K0 HD33894.fit spectrum of HD 33894 MD HD24607.fit spectrum of HD 24607 M HD42537.fit spectrum of HD 42537 MA HD7526.fit spectrum of HD 7526 RO ADC staff NASA/NSSDC 1994 Dec 01 III_179.xml New H-alpha Emmision Stars in the Milky Way. 3180 III/180 SS New H-alpha Emmision Stars in the Milky Way. C B Stephenson N Sanduleak Astrophys. J. Suppl. Ser. 33 459 1977 1977ApJS...33..459S Stars, early-type Stars, emission stars: early-type stars: emission-line, Be stars: spectral classification Data on 455 H-alpha emission stars found in all parts of the Milky Way, virtually all previously unpublished, are tabulated, with newly measured coordinates usually accurate to better than 2". A half-dozen stars appear to have been published previously with erroneous coordinates, or to have been published but omitted from the general catalog by Wackerling (1970). Included among the new stars are known OB stars of the Luminous Stars in the Northern Milky Way survey, from the Hamburg zones, which were originally searched for Half emission at slightly lower spectral resolution than we have used. The stars are in general of early spectral type, and are mostly fainter than the limits of the DM catalogs. The objective-prism plates covered the entire Milky Way within about 10deg of the galactic equator, at a spectral dispersion of about 1000A/mm at H-alpha. This is the catalogue which includes the famous SS 433 object.
The SS(77) catalogue (Table 2 of publication) SS Running number --- RA1900h Right Ascension 1900 (hours) h RA1900m Right Ascension 1900 (minutes) min RA1900s Right Ascension 1900 (seconds) s DE1900- Declination 1900 (sign) --- DE1900d Declination 1900 (degrees) deg DE1900m Declination 1900 (minutes) arcmin DE1900s Declination 1900 (seconds) arcsec RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec l_mV Limit flag (>) on mV --- mV Magnitude based on spectral range 500-600nm, unless the note n_mV indicates 'p' mag n_mV Uncertainty flag (:) or 'p' if mV is a photographic magnitude --- mpg Second magnitude, photographic if followed by 'p' mag n_mpg 'p' if above magnitude is photographic --- Sp Spectral type Spectral types are almost always estimated from 580A/mm blue-region objective-prism plates or quoted from the literature; an absent type means that the star was too faint for our blue plates. The symbols, other than the most standard ones, mean the following: w = H-alpha emission weak, i.e. barely string enough to detect it reliably. s = H-alpha emission strong le = emission lines seen in the blue spectral region OBl = early-type star spectroscopically somewhat less luminous than OB- (in the terminology of the LS catalogue) ce = Balmer continuum in emission r = reddened continuum ov = classification complicated by a spectral overlap on the blue plate --- Remarks Further remarks; the '*' indicates lengthy notes below. --- M.J. Wagner, F. Ochsenbein CDS 1994 Oct 29 UNKNOWN UNKNOWN The catalogue was keypunched at CDS III_180.xml An Atlas of Low-Resolution Near-Infrared Spectra of Normal Stars 3181 III/181 Near Infrared Spectra of Normal Stars An Atlas of Low-Resolution Near-Infrared Spectra of Normal Stars A V Torres-Dodgen W B Weaver Publ. Astron. Soc. Pacific 105 693 1993 1993PASP Atlases Spectra, infrared Stars, normal The authors present digital spectra of O to M stars, luminosity classes V, III, and Ib in the wavelength range 5750-8950 Angstroms, at 15.5 Angstroms resolution. The stars follow well defined morphological sequences in both temperature and luminosity. This wavelength region and resolution, combined with the high sensitivity of silicon-based detectors, are very useful for spectral classification. Details of the observations, identifications of the main spectral features, and spectral lines most sensitive to temperature and luminosity are given in Torres-Dodgen and Weaver (1993).
Fluxes for HD190429A Fluxes for HD13136 Fluxes for HD1326A Fluxes for HD180617 Fluxes for HD190864 Fluxes for HD232979 Fluxes for HD33299 Fluxes for HD46223 Fluxes for HR1017 Fluxes for HR1131 Fluxes for HR1203 Fluxes for HR152 Fluxes for HR1605 Fluxes for HR165 Fluxes for HR1735 Fluxes for HR1749 Fluxes for HR1899 Fluxes for HR21 Fluxes for HR2286 Fluxes for HR2473 Fluxes for HR2615 Fluxes for HR2943 Fluxes for HR3323 Fluxes for HR3975 Fluxes for HR401 Fluxes for HR4189 Fluxes for HR4496 Fluxes for HR45 Fluxes for HR4540 Fluxes for HR4931 Fluxes for HR5291 Fluxes for HR553 Fluxes for HR5993 Fluxes for HR6060 Fluxes for HR6095 Fluxes for HR641 Fluxes for HR6608_A Fluxes for HR6608_B Fluxes for HR6714 Fluxes for HR7387 Fluxes for HR7462 Fluxes for HR7495 Fluxes for HR753 Fluxes for HR7635 Fluxes for HR7796 Fluxes for HR8023 Fluxes for HR8086 Fluxes for HR8313 Fluxes for HR8371 Fluxes for HR8414 Fluxes for HR8428 Fluxes for HR8452 Fluxes for HR8469 Fluxes for HR8622 Fluxes for HR8634 Fluxes for HR8684 Fluxes for HR8694 Fluxes for HR8905 Fluxes for HR996 Fluxes for HSCAS Fluxes for VEGA wavelen Wavelength 0.1nm lflux Log of flux/angstrom --- A. Torres-Dodgen Mont. I.R.A. N. Roman NSSDC/ADC 1994 Dec 05 III_181.xml The Henry Draper Extension Charts: A catalogue of accurate positions, proper motions, magnitudes and spectral types of 86933 stars. 3182 III/182 HDE Charts: positions, proper motions The Henry Draper Extension Charts: A catalogue of accurate positions, proper motions, magnitudes and spectral types of 86933 stars. V V Nesterov A V Kuzmin N T Ashimbaeva A A Volchkov S Roeser U Bastian Astron. Astrophys. Suppl. Ser. 110 367 1995 1995A&AS..110..367N Positional data Proper motions Spectral types catalogs astrometry stars: fundamental parameters stars: variables: general This document is intended to serve as a short description of the data files of the catalogue of 88883 stars of the Henry Draper Extension Charts. Detailed explanation of the Extension, catalogue production and so on may be found in the printed paper referenced above. There are two files comprising the catalogue, namely data file (catalog.dat) and individual remarks file (remarks.txt). The format of the second one is free - it starts with 6-digits HDE number followed by remark text. The catalog.dat file contains 88883 logical records of the length 61 bytes each. A detailed description of the record format is given below. from Paper: The Henry Draper Extension Charts (Cannon et al., 1949), published in the form of finding charts, provide spectral classification for some 87000 stars mostly between 10th and 11th magnitude. This data, being highly valuable, as yet was practically unusable for modern computer-based astronomy. An earlier pilot project (Roeser et al. 1991) demonstrated a possibility to convert this into a star catalogue, using measurements of cartesian coordinates of stars on the charts and positions of the Astrographic Catalogue (AC) for subsequent identification. We present here a final HDEC catalogue comprising accurate positions, proper motions, magnitudes and spectral classes for 86933 stars of the Henry Draper Extension Charts.
The catalogue HD HD number --- m_HD Component identification: A, B... --- n_HD 'R' if individual remark for this star is given in the 'remarks' file --- Sp Spectral class --- Mag Magnitude - photographic or J/V number=2 magnitudes are either the AC B-magnitudes (when PosSource is 'P', 'A' or 'C') or the GSC V/J magnitudes (when PosSource is 'G') mag PosSource Position source flag number=1 Position source is P = PPM (Roeser et al., 1993, "PPM Star Catalogue", Vol. I-IV, Spektrum Akademischer Verlag, Heidelberg C = GSC-AC (Guide Star and Astrographic Catalogues) A = AC (Astrographic Catalogue) G = GSC (Guide Star Catalogue) M = Miscellaneous V = Variables only found in GCVS or CSVS (General Catalogue of Variable stars or Catalogue of Suspected Variable Stars) --- RAh Right Ascension J2000.0 (hours) h RAm Right Ascension J2000.0 (minutes) min RAs Right Ascension J2000.0 (seconds) s DE- Declination J2000.0 (sign) --- DEd Declination J2000.0 (degrees) deg DEm Declination J2000.0 (minutes) arcmin DEs Declination J2000.0 (seconds) arcsec pmFlag If T (TRUE), proper motions are present; if F (FALSE) only the Epoch is present --- pmRA Annual proper motion in RA (if pmFlag=T) arcsec/yr pmDE Annual proper motion in DE (if pmFlag=T) arcsec/yr Epoch Observation epoch in julian years (if pmFlag=F) yr remarks.txt Remarks Francois Ochsenbein CDS 1995 May 18 Siegfried Roeser <S19@MVS.URZ.UNI-HEIDELBERG.DE> III_182.xml An atlas of the infrared spectral region. I. The early type stars (O-G0). 3183 III/183 Atlas of 837.5-877nm spectral region I. An atlas of the infrared spectral region. I. The early type stars (O-G0). Y Andrillat C Jaschek M Jaschek Astron. Astrophys. Suppl. Ser. 112 475 1995 1995A&AS..112..475A Spectra, infrared atlases stars: classification stars: early type infrared: stars The Atlas illustrates the behaviour of early type stars (O, B, A and F type) in the near infrared 8375-8770A region at a resolution of about one A. Intensity tracings of 76 stars are presented. Of these 51 stars cover the spectral range O to G0 and luminosity classes V, III, Ib and Ia. The influence of the rotational velocity is also illustrated as well as the spectra of 19 stars with spectral peculiarities. The complete Atlas is available as a set of FITS files.
List of Stars in the Atlas RemFlag An asterisk indicates an error in the publication --- FileName Name of FITS file with spectrum --- Name Full Star designation --- SpType Spectral Type --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec l_RotVel Limit symbol on Rotational Velocity --- RotVel Projected Rotational Velocity (v.sin(i)) km/s sp01.fit Spectrum of HD 6903 sp02.fit Spectrum of HD 7927 sp03.fit Spectrum of HD 13161 sp04.fit Spectrum of HD 13267 sp05.fit Spectrum of HD 14134 sp06.fit Spectrum of HD 17584 sp07.fit Spectrum of HD 17918 sp08.fit Spectrum of HD 20041 sp09.fit Spectrum of HD 23324 sp10.fit Spectrum of HD 23850 sp11.fit Spectrum of HD 23886 sp12.fit Spectrum of HD 23948 sp14.fit Spectrum of HD 27534 sp15.fit Spectrum of HD 28446 sp16.fit Spectrum of HD 31647 sp17.fit Spectrum of HD 34085 sp18.fit Spectrum of HD 34503 sp19.fit Spectrum of HD 35468 sp20.fit Spectrum of HD 36512 sp21.fit Spectrum of HD 36673 sp22.fit Spectrum of HD 37043 sp23.fit Spectrum of HD 46149 sp24.fit Spectrum of HD 46150 sp25.fit Spectrum of HD 58946 sp26.fit Spectrum of HD 59612 sp27.fit Spectrum of HD 61064 sp28.fit Spectrum of HD 87696 sp29.fit Spectrum of HD 87737 sp30.fit Spectrum of HD 89025 sp31.fit Spectrum of HD 95128 sp32.fit Spectrum of HD 113139 sp33.fit Spectrum of HD 116842 sp34.fit Spectrum of HD 123299 sp35.fit Spectrum of HD 126660 sp36.fit Spectrum of HD 127762 sp37.fit Spectrum of HD 130109 sp38.fit Spectrum of HD 148743 sp39.fit Spectrum of HD 159561 sp40.fit Spectrum of HD 160365 sp41.fit Spectrum of HD 164353 sp42.fit Spectrum of HD 164514 sp43.fit Spectrum of HD 182835 sp44.fit Spectrum of HD 185018 sp45.fit Spectrum of HD 186568 sp46.fit Spectrum of HD 190603 sp47.fit Spectrum of HD 192422 sp48.fit Spectrum of HD 193370 sp49.fit Spectrum of HD 194839 sp50.fit Spectrum of HD 195592 sp51.fit Spectrum of HD 198183 sp52.fit Spectrum of HD 206165 sp53.fit Spectrum of HD 207673 sp54.fit Spectrum of HD 208501 sp55.fit Spectrum of HD 208947 sp56.fit Spectrum of HD 209481 sp57.fit Spectrum of HD 209975 sp58.fit Spectrum of HD 231195 sp59.fit Spectrum of HD 108 sp60.fit Spectrum of WR 5 sp61.fit Spectrum of WR 156 sp62.fit Spectrum of HD 53367 sp63.fit Spectrum of HD 32991 sp64.fit Spectrum of HD 37202 sp65.fit Spectrum of HD 45677 sp66.fit Spectrum of BD+61 154 sp67.fit Spectrum of XX Oph sp68.fit Spectrum of HD 31648 sp69.fit Spectrum of HD 41511 sp70.fit Spectrum of HD 112028 sp71.fit Spectrum of HD 84948 sp72.fit Spectrum of HD 110411 sp73.fit Spectrum of HD 181615 sp74.fit Spectrum of HD 140283 sp75.fit Spectrum of V1974 Cyg sp76.fit Spectrum of PU Vul sp77.fit Spectrum of CH Cyg Francois Ochsenbein CDS 1995 Sep 13 Dr. Y. Andrillat, Laboratoire d'Astronomie, Universite de Montpellier II, URA 1280 et 1281, CNRS, 34095 Montpellier Cedex 5, France UNKNOWN UNKNOWN The magnetic tape was kindly provided to CDS by Dr Y. Andrillat in November 1994. The file "stars" was created from the FITS headers; spectral types and positions were derived from the SIMBAD data-base, and compared with the publication. This comparison led to the two corrections flagged in file "stars", made in agreement with the author. III_183.xml Troisieme Catalogue Bibliographique de Vitesses Radiales Stellaires 3184 III/184 3rd Bibliog. Cat. of Stellar Radial Vel. Troisieme Catalogue Bibliographique de Vitesses Radiales Stellaires M Barbier-Brossat M Petit P Figon Astron. Astrophys. Suppl. Ser. 108 603 1994 1994A&AS..108..603B III/190 : The Wilson-Evans-Batten (WEB) Catalogue Batten A.H. et al., 1989, Pub. Dominion Astroph. Observ. Vol. XVII, p.1-317 =Catalogue <V/64> Duflot et al., Catalogue General de Synthese (in preparation) =Catalogue <III/190> Evans D.S. 1970, Catalogue de Vitesses Radiales Moyennes (private comm.) Van den Berg, 1966, AJ 71, 990, =1966AJ.....71..990V Van den Berg, 1971, AJ 76, 1083 =1971AJ.....76.1083V Wilson R.E., 1953, General Catalogue of Stellar Radial Velocities, Carnegie Inst. of Washington Publ. 601, Washington D.C. =Catalogue <III/21> Radial velocities catalogs techniques: radial velocities stars: kinematics We publish a Bibliographic Catalogue of Stellar Radial Velocities including about 44000 entries for Galactic and Magellanic Cloud stars for the years 1971-1990. The two preceding issues published (1989, A&AS, 80, 67 and 1990, A&AS 85, 885) are mixed with the new data covering the years 1986-1990.
Third bibliographic catalogue of stellar radial velocities HD HD number --- m_HD Multiplicity index on HD number=1 Uppercase letters are used for visual double stars, lowercase letters for spectroscopic double stars. In the second case, the letter 'a' has been replaced by the letter 'i' . The symbol '/' indicates that the measure concerns 2 stars with consecutive HD numbers or that the radial velocity is relative to the measure of the 2 components of the same star. --- DM DM identification (BD, CP, or CD number) --- m_DM Multiplicity index on DM number=1 Uppercase letters are used for visual double stars, lowercase letters for spectroscopic double stars. In the second case, the letter 'a' has been replaced by the letter 'i' . The symbol '/' indicates that the measure concerns 2 stars with consecutive HD numbers or that the radial velocity is relative to the measure of the 2 components of the same star. --- WEB "Catalogue de synthese" reference number=2 Letters W, E and B are related to the "Catalogue General de Synthese" realised from the catalogues of Wilson, Evans and Batten (catalog <III/190>) --- OtherName Other designations --- RAh Right ascension 1950 h RAm Right ascension 1950 min u_RAm Uncertainty flag on right ascension --- DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin n_Vmag 'V' for Variable; '*' if Vmag is a B or photographic magnitude --- Vmag V magnitude (B or photographic magnitude if n_Vmag = *) mag u_Vmag uncertainty flag on Vmag; * indicates very uncertain (::) value --- Sp Spectral type --- RV Heliocentric radial velocity km/s u_RV Uncertainty flag on RV (an unexplained * exists for HD 49212) --- q_RV Quality from A (very good) to E (very poor) --- o_RV Number of (new) measurements --- Rem Remark number=3 The following abbreviations are used: CEPH: Cepheid. The mean velocity is then provided. DBL, TRI, QUAD, MUL: double, triple, quadruple, multiple star respectively DE: eclipsing binary DS, DS1, DS2: spectroscopic binary, with 1 or 2 line systems EM: velocity calculated from emission lines ORB: orbit; the star systemic velocity is provided (unexplained 'E' for Cyg X-1) RRLY: RR Lyrae star. The RR lyrae star gravity center is provided STND: IAU standard star VAR: variable radial velocity, according to the author. --- Disp Dispersion number=4 Dispersion used for the radial velocity determination. If the published velocity is the mean of several velocities obtained with very different dispersions, there is no value of the dispersion. Otherwise, we mention the lowest dispersion used preceded by the symbol <. COR: velocities are measured with a correlation spectrophotometer 0.1nm/mm Ref Reference as Journal Code, Volume, Page number=5 List of abbreviations used for the Journals: AA Acta Astronomica AAP Astronomy and Astrophysics AAPS Astronomy and Astrophysics Supplement Series AAOB Abastumani Astrophysical Observatory Bulletin AFA Arkiv fur Astrophysik AJ Astronomical Journal AN Astronomische Nachrichten AP Astrophysics (URSS) APJ Astrophysical Journal APJS Astrophysical Journal Supplement Series ASS Astrophysics and Space Science AT Annals of the Tokyo Astronomical Observatory BAAA Boletin de la Asociacion Argentina de Astronomia BAAS Bulletin of the American Astronomical Society BAIC Bulletin of the Astronomical Institutes of Czechoslovakia BOTT Boletin de Los Observatorios Tonantzintla y Tacubaya CAO Bulletin de l'Observatoire de Crimee CRAS Comptes Rendus de l'Academie des Sciences, Paris DAO Publications of the Dominion Astrophysical Observatory HA Highlights os Astronomy IAUS International Astronomical Union Symposium IBVS Information Bulletin on Variable Stars JAA Journal of Astrophysics and Astronomy (Inde) JO Journal des Observateurs MAG Mittelungen Astronomische Gesellschaft MAKL Mededelingen van Het Astronomich Institut van de Katholieke Universiteit Leuven MEM Memoirs of the Royal Astronomical Society MES The Messenger (ESO) MN Monthly Notices of the Royal Astronomical Society MNAS Monthly Notices of the Astronomical Society of Sotuh Africa MSAI Memorie della Societa Astronomica Italiana OBS The Observatory PASJ Publications of the Astronomical Society of Japan PASA Publications of the Astronomical Society of Australia PASP Publications of the Astronomical Society of Pacific PCAO Publication Crimean Astrophysical Observatory PDDO Publications of the David Dunlap Observatory POAS Publications de l'Observatoire Astronomique de Strasbourg POCC Observatorio Astronomico Nacional, Cerro Calan, Publicaciones POGB Publications de l'Observatoire de Geneve, Serie B RASC Journal of the Royal Astronomical Society of Canada RASV Ricerche Astronomiche Specola Vaticana RGOA Royal Greenwich Observatory Annals RMAA Revista Mexicana de Astronomia y Astrofisica ROB Royal Observatory Bulletin SA Soviet Astronomy SAL Soviet Astronomy - Letters SAOC South African Astronomical Observatory Circulars VA Vistas in Astronomy --- Year Year of publication --- Rem2 Remarks. '*' indicates remark in note number=6 Remarks: - Ma 260 in AAP 17, 253-1972. We deleted the BD identification given by the author because it doesn't correspond to the star coordinates - LTT 664 = CD-44 334 instead of CD-44 344 in AJ 84, 1553-1979 - Fl 770 in POAS 2, 1-1972. The published coordinates don't correspond to those of star CP-74 106. We deleted this identification. - HD 11154 = HR 530 instead of HD 11155 in APJS 62, 147 - HD 22484 = BD-0 572 instead of BD+0 572 in AAPS 71, 253 - vB 188 instead of vB 178 in AJ 88, 844-1983 from published coordinates - HD 36486 in APJ 214, 759-1977. The systemic velocity +118.3 published seems wrong compared with other publications. This velocity might be +18.3 - Gl 234A instead of 243A in APJS 314, 272-1987 - NGC 2287 c4 = HD 49105 in AAPS 62, 301-1985. The coordinates and the spectral type published in the paper don't correspond to those of HD. We deleted this identification. - HD 86612 instead of HD 86162 in AAPS 63, 87-1986 - CC Com in PASP 89, 684-1977. The coordinates are different from those of the "Catalogue d'Etoiles Variables" by Kukarkin. - HD 112211 instead of 12211 in AJ 89, 1897-1984 - HD 119191 instead of 19191 in AJ 89, 1897-1984 - CD-29 10863 instead of CD-20 10863 in AJ 89, 1897-1984 - HD 129981 instead of HD 129881 in MN 159, 67-1972 - HD 151985 instead of 151895 in APJS 64, 487-1982 - Case 437 in AJ 81, 364-176. We adopted the coordinates from Case catalogue which differ slightly from the published ones. - CD-23 13997 instead of CP-23 13997 in MN 158, 85-1972 - CD-23 13998 instead of CP-23 13998 in MN 158, 85-1972 - CD-35 12911 in POCC 2, 40-1970. The author coordinates differ from those indicated in SIMBAD, which we have adopted. - APJS 73, 843-1990. There is some confusion between the corresponding numbers. cya 51=CCS 2866=nb 201 cya 50=CCS 2862=nb 202 cya 77=CCS 2873 cya 76=CCS 2874 - BD+15 4915 instead of BD+15 4914 in PASP 97, 1086-1985 - MN 230, 273-1988 = DAO 16, 297-1988. The stars in these two articles are identical. We only retained the DAO paper, which was earlier. - AJ 87, 1679-1982 and AJ 94, 1600-1987. Some stars are in the two papers with the same data. In this case, the second publication was ignored. - APJS 64, 487-1987. We detected errors in the mean radial velocities, and we recalculated mean RV - AAPS 48, 409-1982. As requested by the authors, the radial velocities published there replace those form AAPS 13, 173, 1974: the latter data were removed from the catalogue. - AJ 93, 463-1987. These stars are from the study of van den Berg (1971), and they differ from those indicated in SIMBAD which are from an earlier publication of the same author (1966). - Corrections have been made in the papers AAPS 43, 297-1981, AAPS 49, 483-1982, AAPS 58, 435-1984 et AAPS 68, 515-1987, with the authorisation of the authors. - AAPS 4, 231-1971. The corrections published by the author in the erratum in AAPS 16, 277-1974 have been taken into account. --- Patricia Bauer CDS 1995 Jan 05 III_184.xml A Search for Jupiter-Mass Companions to Near-By Stars 3185 III/185 Search for Jupiter-Mass Companions A Search for Jupiter-Mass Companions to Near-By Stars G A H Walker A R Walker A W Irwin A M Larson S L S Yang D C Richardson Icarus 116 359-375 1995 1995Icar..116..359W Radial velocities Planets From 1980 to 1992, the radial velocities of 17 bright solar-type dwarf and 4 subgiant stars were monitored at the Canada-France-Hawaii 3.6-m telescope (CFHT).
The experimental technique, in which lines of the 870 nm 3-0 vibration-rotation band of hydrogen fluoride are imposed in absorption on the stellar spectra to act as wavelength fiducials, is capable of measuring long-term changes in the velocity of a star with a precision near 15 m/s from a single spectrum. For comparison, the orbit of the Sun about the barycentre, which is dominated by the motion of Jupiter, has a period of 11.9 years with an amplitude of some 13 m/s. Thus, by making several observations per year, we could have detected the reflex motion caused by a Jupiter-mass planet orbiting a nearby star provided the orbital plane was close to the line of sight. To date, this planetary search has been the only long-term program on the CFHT. Between three and six pairs of nights per year were allocated over twelve years, apart from a single gap of six months in 1983. The 15 m/s precision per observation was achieved to a limiting I magnitude of 4 for exposures of typically less than half an hour. The program was completed in 1992. In the published paper the analysis of the 1082 individual differential velocities that are cataloged here is presented.
Catalog of precise radial velocities of 21 near-by stars HR Bright Star Catalog number --- HD HD Catalog number --- Name Star name This is specified for all stars except HR 8832 which does not have a name designated in the Bright Star Catalog. --- RJD Epoch (Barycentric JD - 2440000) d PRV Precise Radial Velocity m/s ERR Internal (standard) error of PRV m/s A. W. Irwin University of Victoria 1995 May 08 III_185.xml Intrinsic energy distribution in stars at 320-760 nm. 3186 III/186 Energy distribution in stars at 320-760 nm Intrinsic energy distribution in stars at 320-760 nm. L N Knyazeva A V Kharitonov Astron. Zh. 73 571 1996 1996AZh....73..571K Stars, normal Spectrophotometry The intrinsic energy distribution for 41 spectral subclasses in the range of wavelengths of 320-760 nm are derived in the following way: (1) The sources of the spectrophotometric data were taken from three catalogues published in FSU (Kharitonov et al. 1988, Glushneva, ed., 1982, Alekseeva et al. 1992), containing energy distributions of about 2000 stars of different spectral types. (2) MK spectral classes were taken from the Bright Star Catalogue (Hoffleit 1982; hereafter BSC). The paper by Gray and Garrison (1987) was took into account to examine the influence of errors in spectral classification. (3) The quality of stars selected for each subclass was estimated by comparison of the observed and synthetic (U-B) and (B-V) color indices calculated for our energy distributions. The results have been published by Knyazeva and Kharitonov (1993, 1994a, 1994b, 1996a, 1996b)
Intrinsic energy distribution for spectral subclasses (relative to maximum) Lambda Spectral line wavelength 0.1nm E(B5V) Intrinsic energy for B5V --- E(B7V) Intrinsic energy for B7V --- E(B8V) Intrinsic energy for B8V --- E(B9V) Intrinsic energy for B9V --- E(B9.5V) Intrinsic energy for B9.5V --- E(A0V) Intrinsic energy for A0V --- E(A1V) Intrinsic energy for A1V --- E(A2V) Intrinsic energy for A2V --- E(A3V) Intrinsic energy for A3V --- E(A4V) Intrinsic energy for A4V --- E(A5V) Intrinsic energy for A5V --- E(A7V) Intrinsic energy for A7V --- E(A3IV) Intrinsic energy for A3IV --- E(A7IV) Intrinsic energy for A7IV --- E(F0V) Intrinsic energy for F0V --- E(F5V) Intrinsic energy for F5V --- E(F6V) Intrinsic energy for F6V --- E(F7V) Intrinsic energy for F7V --- E(F8V) Intrinsic energy for F8V --- E(F0IV) Intrinsic energy for F0IV --- E(F2IV) Intrinsic energy for F2IV --- E(F5IV) Intrinsic energy for F5IV --- E(G0V) Intrinsic energy for G0V --- E(G2V) Intrinsic energy for G2V --- E(G5V) Intrinsic energy for G5V --- E(G8V) Intrinsic energy for G8V --- E(G7III) Intrinsic energy for G7III --- E(G8III) Intrinsic energy for G8III --- E(G9III) Intrinsic energy for G9III --- E(K0III) Intrinsic energy for K0III --- E(K1III) Intrinsic energy for K1III --- E(K2III) Intrinsic energy for K2III --- E(K3III) Intrinsic energy for K3III --- E(K4III) Intrinsic energy for K4III --- E(K5III) Intrinsic energy for K5III --- E(M0III) Intrinsic energy for M0III --- E(M1III) Intrinsic energy for M1III --- E(M2III) Intrinsic energy for M2III --- E(M3III) Intrinsic energy for M3III --- E(M4III) Intrinsic energy for M4III --- E(M5III) Intrinsic energy for M5III --- Veta Avedisova INASAN 1996 Dec 30 III_186.xml International Ultraviolet Explorer Atlas of B-type Spectra from 1200 to 1900 A 3188 III/188 IUE Atlas of B-Type Stellar Spectra International Ultraviolet Explorer Atlas of B-type Spectra from 1200 to 1900 A N R Walborn J W Parker J S Nichols NASA Reference Publication #1363 ??? ??? 1995 1995N95-28328.....W International Ultraviolet Explorer Atlas of B-type Spectra from 1200 to 1900 A J W Parker N R Walborn J S Nichols T R Gull Bull. American Astron. Soc., 186, #22.21 ??? ??? 1995 1995AAS...186.2221P Stars, B-type Spectra, ultraviolet Atlases The IUE Atlas of B-type Stellar Spectra is an atlas of B-type spectra consisting of short-wavelength, high-resolution data from the International Ultraviolet Explorer archive, designed to complement the widely used O-star atlas from the same source (Walborn, Nichols-Bohlin, & Panek 1985, NASA Reference Publication 1155). The atlas presented here completes the OB natural group, i.e., to spectral type B3 for the main sequence and giants, type B5 at class Ib, and B8 at Ia, which is also the most relevant domain for stellar-wind effects among normal B-type spectra.
A primary objective of the IUE Atlas of B-type Stellar Spectra is to chart in detail the gradual disappearance of the stellar-wind features in normal spectra as a function of spectral type and luminosity class. As in the O-star atlas, which first demonstrated the strong correlation between the optical spectral types and the UV wind behavior in the majority of the stars, the principal selection criterion was the existence of high-weight optical spectral classifications, which are quoted here without any revisions based upon the UV data. Some peculiar categories also are presented including a number of hypergiants, stars of types BN/BC (and including three of type O9.7 acquired since the O Atlas), and stars with enhanced winds. 86 images have been selected from the IUE archive for the atlas. The processing and presentation is as similar as possible to the O-star atlas, with the SWP data (roughly 1200-1900 angstrom range) rectified and rebinned to a uniform resolution of 0.25 angstrom. The conclusions from the B Star Atlas are similar to those from the O Star Atlas, namely, that the UV stellar-wind features display strong systematic trends as a functions of spectral type and luminosity class, and a high degree of correlation with the optical classifications as the winds decline toward the later types. A somewhat higher rate of exceptions to these correlations can be recognized among the B spectra (11%) than the O (2%), but they remain a small fractions of the total sample and do not prevent clear delineation of the normal behavior. Indeed, it is only as a result of the latter that the exceptions can be identified and described.
Star IDs, Spectral Types, IUE image numbers, PI names, atlas plate numbers ID HD/HDE or Sanduleak (Sk) number of star --- Name Name of star --- Sp Optical spectral classification --- SWP_num SWP camera image number of observation --- PI_name Name of the IUE principal investigator --- Plate_1 First atlas plate showing spectrogram Location of of the spectrogram in the printed atlas. Each plate covers two pages in the atlas (first page covers 1200-1500 A, and the second page covers 1500-1900 A). Some spectrograms appear on more than one plate. --- Plate_2 Second atlas plate showing spectrogram --- Plate_3 Third atlas plate showing spectrogram --- Fluxes and data quality flags ID HD/HDE or Sanduleak (Sk) number of star There are 800 records for each star, and the ID appears at the beginning of each record for a given star. --- lambda Wavelength of first flux/quality pair The quoted wavelength value is the wavelength of the flux_1 and qual_1 data pair. The wavelengths for the subsequent flux/qual data pairs in the record are in increments of 0.025 nm. 0.1nm flux_1 Normalized flux at wavelength=lambda See Appendix A: "Data Preparation" for a brief description of how the normalized flux was calculated. --- qual_1 Data quality flag associated with flux_1 See Appendix A: "Data Preparation" for a brief description of how this normalized quality factor was calculated. --- flux_2 Normalized flux at wavelength=lambda+0.025 nm --- qual_2 Data quality flag associated with flux_2 --- flux_3 Normalized flux at wavelength=lambda+0.050 nm --- qual_3 Data quality flag associated with flux_3 --- flux_4 Normalized flux at wavelength lambda+0.075 nm --- qual_4 Data quality flag associated with flux_4 --- Splice points of spectra ID HD/HDE or Sanduleak (Sk) number of star There are 13 records for each star, and the ID appears at the beginning of each record for a given star. --- splice1 First splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice2 Second splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice3 Third splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice4 Fourth splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice5 Fifth splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice6 Sixth splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice7 Seventh splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm splice8 Eighth splice point Splice points are the wavelength values where overlap of successive orders of the IUE spectrum have been spliced together. These values come in four pairs per record, where for each pair: The first wavelength the beginning of the next (higher) order, and The second wavelength of the end of the previous (lower) order. 0.1nm Joel W. Parker Code 680/GSFC 1995 Aug 07 UNKNOWN UNKNOWN A. Data Preparation: This section briefly describes the steps involved in selecting and processing the data comprising this atlas. The following description was extracted from an edited version of Walborn et al. (1995). A.1 Selection As in the O Atlas, the principal selection criterion was the existence of high-weight optical spectral classifications, which are quoted here without any revisions based upon the UV data. A.2 Processing The processing of the spectral data presented in this Atlas is substantially similar to that used for the O Atlas. The high-resolution SWP data were retrieved from the National Space Science Data Center in their original IUESIPS processed form. Sample wavelength and a data quality indicator were also included. The spectral data were then further reduced at the IUE Data Analysis Center. Processing then proceeded through the following steps: 1. The background was smoothed and subtracted from the on-order signal to yield the net spectrum. 2. A "ripple" correction was applied to adjust for systematic variation along each order caused by the varying sensitivity of the echelle grating. The orders were then spliced at the points where sensitivities of adjacent orders are equal. These points of overlap are listed in the second file. The spectrum was then resampled to 0.25 A resolution: The complete concatenated spectrogram was rebinned to a uniform resolution of 0.25 A. The resampled points were computed from a weighted average of the original points, the weight being based on the fraction of the original bin that falls within the 0.25 A window centered at the new wavelength point. A weight of zero was assigned to any original point possessing an IUESIPS quality flag indicating reseau contamination, saturation, or a particle hit event. The new sample points are spaced evenly at 0.25 A intervals from 1150 to 1950 A. A new quality flag was derived for each rebinned point, computed as the sum of the weights for the original samples contributing to the new point. A minor error in this resampling algorithm was detected after preparation of the O Atlas in 1985. The end points of each bin overlapped by one extracted point, so that these end points were included in two bins. The error was subsequently corrected and it does not affect the data in the present Atlas. 3. The resampled spectrum was then rescaled in order to locate the stellar continuum at an approximately uniform level: Each rebinned spectrogram was normalized by dividing by a "continuum spectrum" created from a highly smoothed version of itself. In a few cases in which the resulting normalization was unsatisfactory, with remaining large-scale structure in the continuum, the normalization was redone manually. Similarly, the data-quality flags were normalized to remove the effect of the decreasing spectral dispersion at longer wavelengths, which results in a smaller number of original samples within each 0.25 A bin. Large geocoronal Lyman-alpha and particle-hit spikes were manually removed from the data, and in a few cases of low signal at the shorter wavelengths, noise spikes were truncated at the borders of the frame [normalized flux values of 0 and 2.5] to avoid overwriting the adjacent spectrograms. [This truncation also exists for the archived electronic version of these data, so many spectra will have chopped spikes, particularly in the region around Lyman-alpha.] The data-quality flags are coded as numbers between 0 and roughly 1: small downward spikes are produced when a few of the points in the bin are contaminated with a reseau mark, and large downward spikes are produced when all of the points in the bin have reseau or other contamination. Extracted spectral data points are flagged as contaminated by a reseau mark if the mark falls near or on the spectral order. It is possible for one or more rebinned points to have a near zero quality flag but the spectral data are unaffected by the reseau mark. III_188.xml MK Spectral Classifications - Twelfth General Catalog 3189A III/189A General Catalogue of MK Classifications MK Spectral Classifications - Twelfth General Catalog W Buscombe B E Foster Northwestern University, Evanston Illinois ??? ??? 1995 1995msct.book.....B Spectral types A file of MK spectral types and UBV photometry maintained at Dearborn Observatory is presented here. It is based on an extensive literature search and is up to date as of early 1995.
The data file Data for IC1805 Data for Orion trapezium Data for NGC 3293 Data for NGC 6087 Data for NGC 6475 (M 7) Data for NGC 752 Data for Orion association Data for upper Sco and Oph assoc. Data for Small Magellanic Cloud id Identification for star --- RAh Right Ascension (2000) hour h RAm Right Ascension (2000) minute min DE- Declination sign --- DEd Declination (2000) degree deg DEm Declination (2000) minute arcmin u_DEm DEm uncertain --- Sp MK type --- r_Sp Asterisk = type from definers of MK --- mag< Brackets mean average over cycle --- V V magnitude mag mag> Brackets mean average over cycle --- B-V< Brackets mean average over cycle --- B-V B-V color mag B-V> Brackets mean average over cycle --- U-B U-B color mag uncer Questions --- name Alternate identification, usually HD --- Nancy G. Roman ADC/SSDOO 1997 Apr 08 III_189A.xml Radial velocities. The Wilson Evans Batten catalogue WEB (Wilson Evans Batten) Catalogue 3190B III/190B WEB Catalog of Radial Velocities Radial velocities. The Wilson Evans Batten catalogue WEB (Wilson Evans Batten) Catalogue M Duflot P Figon N Meyssonnier Astron. Astrophys. Suppl. Ser. 114 269 1995 1995A&AS..114..269D I/211 : CCDM Catalogue: Dommanget J., Nys O., 1994, Comm. de l'Observatoire Royal de Belgique, serie A, no 115 I/196 : Turon C.,1992, the HIPPARCOS Input Catalogue, ESA SP-1136 III/21 : Wilson R.F., 1953, "General Catalogue of stellar radial velocity", Carnegie Institution of Washington Publ. 601 III/47 : Evans D.S, 1967, "Catalogue of stellar radial velocities", in IAU Symp. 30, 57, ed. A.H. Batten & J.F. Heard, Academic Press V/64 : Batten A.H., Flechter J.M., MacCarthy D.G., 1989, Publ. Dominion Astrophys. Obs. 17 Radial velocities techniques: radial velocities catalogs stars: kinematics We give a common version of the two catalogues of Mean Radial Velocities by Wilson (1953; catalogue <III/21>) and Evans (1978; catalogue <III/47>) to which we have added the catalogue of spectroscopic binary systems (Batten et al. 1989; catalogue <V/64>). For each star, when possible, we give: 1) an acronym to enter SIMBAD (Set of Identifications Measurements and Bibliography for Astronomical Data; see <http://cdsweb.u-strasbg.fr/Simbad.html>) of the CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the number HIC of the HIPPARCOS catalogue (Turon 1992; catalogue <I/196>). 3) the CCDM number (Catalogue des Composantes des etoiles Doubles et Multiples) by Dommanget & Nys (1994; catalogue <I/211>). For the cluster stars, a precise study has been done, on the identification numbers. Numerous remarks point out the problems we have had to deal with. => In the paper, and in the file "annex2", the equinox of the coordinates is 1950, whereas 2000 equinox is used for the web catalog; => In the paper, read "Wilson (1953)" instead of "Wilson (1963)"
Catalogue WEB (version 2, February 1996) HD Number in the Henry Draper Catalogue <III/135> --- m_HD Multiplicity note the following symbols are used: / two successive HD numbers for only one line (see annex2, part 2-I) $ the radial velocity is that of a sub system (see article section 3.4c) --- RAh Right ascension 2000, from SIMBAD/CDS (Nov/Dec 1995), when they exist h RAm Right ascension 2000 (minutes and tenth of minutes) min DE- Declination sign --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin n_SIMBAD # for coordinates not in SIMBAD, precessed by us --- Vmag Visual or photoelectric magnitude mag n_Vmag Note on Vmag the following symbols are used: * when magnitude is photographic not visual V for variables stars : this symbol exists in Evans catalogue (probably for uncertain value) --- Sp Spectral Type column 40 contains, if Wilson luminosity: c: supergiant d: dwarf g: giant s: subgiant t: subdwarf or ":" for HD 12938 for uncertain magnitude --- RV Radial Velocity. km/s u_RV Uncertainty on RV ":" for doubtful RV "*" from original catalogue of Batten (probably for inaccurate RV) --- n_RV Remark on RV nature and observations "e" for emission radial velocity "G" RV of the gravity center for double or multiple system (see article section 3.4) "g" RV of the gravity center for a sub-system (see article section 3.4) --- q_RV Quality of the radial velocity (I for insufficient information) --- o_RV Total number of plates on which the radial velocity is based. number of plates or "N" (in column 53) undetermined but large number of observations or "?" (in column 53) unknown number of observations --- DM DM identification the first two bytes designate the Durchmusterung BD Bonner Durchmusterung (DE >= -22) CD Cordoba (-22> DE >-52) CP Cape (DE <= -52) (small letters for CD or CP indicate case where the HD convention is not followed) --- Names Identifications found in the different catalogues (Wrong identifications are sometimes omitted) GC Number in the General Catalogue (B. Boss; catalog <I/113>) A, ADS Aitken number (the additional symbols A, B... indicating the components ) AC Astrographic Catalogues....... AGK2 Catalogue AGK2 Bd Bordeaux Astr Chart 516,Star 209 Brun Brun,A.,1935,Publ. Obs. de Lyon 1,12 BSD Kapteyn, Stars in Selected Areas C Cincinnati Publications, vol. 18 CC Cincinnati Publications, vol. 20 F Furuhjelm Feige Feige,J.,1958,ApJ 128,267 GCRV General Catalogue of Radial Velocity (Wilson, catalog <III/21>) Hil Hiltner,W.A.,1956,ApJS 2,389 I First Index Catalogue of Nebulae II Second Index Catalogue of Nebulae J Jonckheere LDS Luyten,W.J., Double Stars Lee Lee,O.J., Red Stars from Dearborn Objective Prism Survey LMC-N Henize 1955, Emission nebulae in the Large Magellanic Cloud LPM Luyten,W.J., Proper Motion Stars L,LTT,Luy Luyten,W.J., Miscellaneous lists LYe Luyten, W.J. MCC Vyssotsky,A.N., MCC number (McCormick Observatory) MSB Merrill,C.G., Sanford,R.F., Burwell,C.G. MWC Merrill,P.W., Burwell,C.G.,Mount Wilson Catalogue Mc Leander McCormick Observatory, Faint Dwarf Stars N,NGC Dreyer, New General Catalogue of Nebulae and Clusters NGP Upgren,A.R. Jr. Stars in North Galactic Pole NSV Kholopov,P.N., New Catalogue of Suspected Variable Stars PK Perek,L., Kohoutek,L. Catalogue of Galactic Planetary Nebulae (Prague, 1967) Ross Ross,F.E., Faint Proper Motion Stars T Toulouse Tr Trumpler,R.W., Stars in Open Clusters V Variable stars Vyss Vyssotsky,A.N., MCC number (McCormick Observatory) Wolf Max Wolf, Faint Proper Motion Stars --- Observ Observatories contributing to the mean radial velocity For the catalogue Wilson, the observatories are indicated by the following symbols: A Allegheny B Bonn Bb Berlin-Babelsberg C Cape Cd Cordoba D Dunlap F Fehrenbach (Haute-Provence) Hd Harvard L Lick Lw Lowell M Moore General Catalogue Md McDonald Mi Michigan O Ottawa Pm Postdam Pn Perkins S Simeis V Victoria Vn Vienna W Mount Wilson Wc Mount Wilson (9-feet coude) Y Yerkes --- n_CCDM CCDM symbols (* published, + private com.) --- CCDM Number in the CCDM <I/221> Catalogue --- orb "*" for visual orbit --- bin "#" code for visual binary (see article section 3.3b) --- GCRV Number in Wilson's General Catalogue of Radial Velocity <III/21> --- SIMBAD Identification allowing SIMBAD access --- Note Remark, see annex2 the letters A - K send to different error types explained (in French) in annex2 file. The letters mean: A : stars from Batten <V/64> without V0 value B : miscellaneous notes C : errors related to star identifications in original or machine-readable catalogues D : stars for which Evans <III/47> did not take Wilson's results into account E : Spectroscopic binaries with V0 without signification from objective prism by Gieseking (=1981A&AS...43...33G; =1984A&AS...57...99G) F : Interversion in HD or BD components G : Stars from Wilson <III/21> and Evand <III/47> removed in the WEB. H : Astrometric binaries I : Systems having a "/" in HD, but where the A component has the largest HD number J : velocities from Heard (1956PDDO....2..105H) not in Evans catalogue <III/47> K : simultaneously spectroscopic and visual binaries, where it is difficult to identify which component is the spectroscopic binary. --- HIC Hipparcos <I/196> number --- Catal Catalogue where are extracted the data W = Wilson <III/21> E = Evans <III/47> B = Batten <V/64> (1989, Publ. D.A.O. XVII,1) --- n_Catal Contributions to the RV E (in column 133) if a precedent mean RV is found in Evans catalogue W (in column 134) if a precedent mean RV is found in Wilson catalogue --- WEB WEB number (provisional) --- Patricia Bauer, Francois Ochsenbein CDS 1998 Apr 03 Meyssonnier N. <meyssonnier@obmara.cnrs-mrs.fr> Duflot M. <duflot@observatoire.cnrs-mrs.fr> UNKNOWN UNKNOWN * December 1995: first version (20795 stars) * February 1996: corrections detailed in file "changes" (20793 stars) * March 1998: version 6 of the WEB installed as catalogue III/190B (see detailed corrections in file "changes") III_190B.xml Les vitesses radiales du PPO de FEHRENBACH, annees 1955-68 (Radial Velocities from Small Objective Prism by FEHRENBACH, in years 1955-68) 3192 III/192 Radial Velocities measured at PPO by FEHRENBACH Les vitesses radiales du PPO de FEHRENBACH, annees 1955-68 (Radial Velocities from Small Objective Prism by FEHRENBACH, in years 1955-68) Ch Fehrenbach M Duflot V Genty G Amieux Bull. Inf. CDS 48 11 1996 1996BICDS..48...11F III/190 : Wilson-Evans-Batten (WEB) catalogue Radial velocities The radial velocities measured on plates taken with Small Objective Prism instrument at Observatoire de Haute-Provence (OHP), and published in the years 1955-1968, have been improved; the radial velocities derived from a single plate measurement have been eliminated. These corrections imply modifications in Evans's catalogue <III/47>; the modifications have been reported in the "WEB" catalogue <III/190> (see Duflot et al., =1995A&AS..114..269D)
The corrected radial velocities HD HD number --- m_HD '/' when 2 consecutive HD numbers merged --- RAh Right Ascension 1950 (hour) h RAm Right Ascension 1950 (minute) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degree) deg DEm Declination 1950 (arcminute) arcmin Pmag Photographic magnitude from AGK2 (see n_Pmag) mag n_Pmag '*' when Pmag not from AGK2 --- Sp Spectral type (from the authors) --- RV Radial velocity km/s q_RV Quality of RV number=1 the quality index is (see Publication OHP, Vol 4, no 12): A probable error <= 2.5 km/s B 2.5 < probable error <= 5.0 km/s C 5.0 < probable error <= 10.0 km/s D 10.0 < probable error --- o_RV Number of RV measurements --- Name Other designation number=2 the other designation include: BD = Bonner Durchmusterung (catalog <I/122>) AGK2 = Zweiter Kalalog der astronomische Gesellschaft BSD = Bergedorfer Spektral Durchmusterung UBV = Blanco et al. UBV catalog (Publ. U.S. Naval Obs., Second Ser., 21) --- Field Field number number=3 the field numbers are the following: 1 : 4x4 degrees centered on HD 183537 (Champ 5) 2 : 4x4 degrees centered on HD 191243 (Champ 6) 3 : 4x4 degrees centered on HD 191243 (Champ 6OB) 4 : 4x4 degrees centered on HD 200120 (Champ 7) 5 : 4x4 degrees centered on HD 210855 (Champ 8) 6 : 4x4 degrees centered on HD 225180 (Champ 9) 7 : 4x4 degrees centered on HD 225180 (Champ 9OB) 8 : 4x4 degrees centered on HD 12953 (Champ 10) 9 : 4x4 degrees centered on HD 12953 (Champ 10OB) 10 : 4x4 degrees centered on HD 24431 (Champ 11) 11 : 4x4 degrees centered on HD 31617 (Champ 12) 12 : 4x4 degrees centered on HD 42784 (Champ 14) 13 : 4x4 degrees centered on HD 47240 (Champ 15) 14 : 4x4 degrees centered on HD 47240 (Champ 15OB) 15 : 4x4 degrees centered on HD 9878 (Champ I) 16 : 4x4 degrees centered on HD 11857 (Champ J) 17 : 4x4 degrees centered on HD 14817 (Champ K) 18 : 4x4 degrees centered on HD 15449 (Champ L) 19 : 4x4 degrees centered on HD 17086 (Champ M) 20 : 4x4 degrees centered on HD 40297 (PaO) 21 : 4x4 degrees centered on BD+17 712 (delta Tau) 22 : 4x4 degrees centered on HD 107966 (Com Ber) 23 : 4x4 degrees centered on HD 191610 (28 Cyg) 24 : 4x4 degrees centered on HD 193237 (P Cyg) 25 : 4x4 degrees centered on HD 14433 (h+chi Per) 26 : 4x4 degrees centered on HD 6382 (SA 8) 27 : 4x4 degrees centered on HD 19536 (SA 9) 28 : 4x4 degrees centered on HD 221039 (SA 19) 29 : 4x4 degrees centered on HD 9996 (SA 21) 30 : 4x4 degrees centered on HD 29882 (SA 24) 31 : 4x4 degrees centered on HD 84219 (SA 29) 32 : 4x4 degrees centered on HD 93013 (SA 30) 33 : 4x4 degrees centered on HD 198414 (SA 40) 34 : 4x4 degrees centered on HD 16397 (SA 46) 35 : 4x4 degrees centered on BD+30 2176 (SA 55) 36 : 4x4 degrees centered on HD 114172 (SA 57) 37 : 4x4 degrees centered on HD 189943 (SA 64) 38 : 4x4 degrees centered on HD 218199 (SA 67) 39 : 4x4 degrees centered on HD 8110 (SA 69) 40 : 4x4 degrees centered on HD 44033 (SA 74) 41 : 4x4 degrees centered on HD 57049 (SA 75) 42 : 4x4 degrees centered on BD+14 4768 (SA 90) 43 : 4x4 degrees centered on BD+14 4967 (SA 91) 44 : 4x4 degrees centered on HD 18286 (SA 94) 45 : 4x4 degrees centered on HD 206660 (SA 113) 46 : Stars common to fields 18 & 19 (L and M) 47 : Stars common to fields 18 & 25 (L and h+chi Per) 48 : Stars common to fields 19 & 27 (M and SA9) --- POHP Publication number number=4 the numbers refer to the following publications: 1 : OHP3 N 41 (1955) 9 : OHP6 N 16 (1962) 2 : OHP3 N 49 (1956) 10 : OHP6 N 36 (1963) 3 : OHP4 N 12 (1957) 11 : OHP7 N 8 (1962) 4 : OHP4 N 34 (1958) 12 : OHP8 N 25 (1966) 5 : OHP4 N 55 (1959) 13 : OHP9 N 38 (1968) 6 : OHP5 N 3 (1959) 7 : OHP5 N 54 (1961) 8 : OHP6 N 8 (1963) --- Number Order number in publication --- Francois Ochsenbein CDS 1996 Apr 02 M. Duflot, Marseille Observatory <duflot@obmara.cnrs-mrs.fr> III_192.xml Chemical Abundances in Late-Type Stars 3193 III/193 Chemical Abundances in Late-Type Stars Chemical Abundances in Late-Type Stars F Thevenin Bull. Inf. CDS 49 ??? ??? in press 1998BICDS.in.press.T III/200 : Catalogue of [Fe/H] (Cayrel de Strobel+, 1997) =1992A&AS...95..273C Cayrel de Strobel et al.'s 1992 catalogue. (See cat. <III/200>) 578 =1990A&A...236L...5M Molaro P., Bonifacio P., 1990, A&A 236, L5-8 579 =1993A&A...275..101E Edvardsson B., Andersen J., Gustafsson B., Lambert D., Nissen P., Tomkin J.,1993,A&A 275,101 580 =1990MNRAS.247..132A Adelman S.J., Philip A.G.D., 1990, MNRAS 247, 132 581 =1993A&A...272..116S Spite F., Barbuy B., Spite M., 1993, A&A 272, 116 582 =1993AJ....106.1490K Kraft R.,Sneden C., Langer G., Shetrone M., 1993, AJ 106, 1490 583 =1991AJ....102..303R Ryan S., Norris J. , Bessel M., 1991, AJ 102, 303 584 =1992A&A...263..249S Smith G., Lambert D., Ruck M., 1992, A&A 263, 249 585 =1991A&AS...88..365F Francois P., Huile S., 1991, A&AS 88, 365 586 =1994A&AS..103..321N North P., Berthet S., Lanz T., 1994, A&AS 103, 321 587 =1994AJ....107.1773S Sneden C., Kraft R., Langer G., Prosser C., Shetrone M., 1994, AJ 107, 1773 588 =1994ApJS...91..749M McWilliam A., Rich M., 1994, AJ 91, 749 589 =1989ApJS...71..559L Luck E., Bond H., 1989, ApJS 71, 559 590 =1990ApJ...357..188L Luck E., Bond H., Lambert D., 1990, ApJ 357, 188 591 =1994AJ....108..285B Beveridge R., Sneden C., 1994, AJ, 108, 285 592 =1991ApJ...373..105P Pritchet J., Glaspey W., 1991, ApJ 373, 105 593 =1994AJ....108..271G Glaspey W., Pritchet J., Stetson P., AJ 108, 271 594 =1980A&AS...41..397C Castley J.C., Watson R.D. 1980, A&AS 41, 397 595 =1994AZh....71..638R Rachkovskaya T.M., Astronomy reports 38, 566 596 =1994ApJ...435..797D Drake J., Lambert D., 1994, ApJ 435, 797 597 =1994A&A...283..911G Gratton R., Contarini G., 1994, A&A 283, 911 598 =1994A&A...290..885P Primas F., Molaro P., Castelli F., 1994, A&A 290, 885 599 =1994A&A...287..927G Gratton R., Sneden C., 1994, A&A 287, 927 600 =1995A&A...293...75E Edvardsson B., Pettersson, Kharrazi M., Westerlund B., 1995, A&A 293, 75 601 =1995A&A...293..347H Hill V., Andrievsky S., Spite M., 1995, A&A 293, 347 602 =1989ApJS...71..559L Luck E., Bond H., ApJS 71, 559 Abundances Effective temperatures Stars, late-type stars: atmospheres stars: abundances The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. <III/200>). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.
Abundances from Li to Eu for individual stars Cluster Name of cluster --- Star Star name --- theta Effective temperature (5040/T) (Sun=0.87) K-1 logg Gravity (Sun=4.4) [cm/s2] zeta Microturbulence velocity (Sun=1.1) km/s [Li] Lithium (Z= 3) abundance [Sun] [O] Oxygen (Z= 8) abundance (Sun=8.92) [Sun] [Na] Natrium (Z=11) abundance (Sun=6.28) [Sun] [Mg] Magnesium (Z=12) abundance (Sun=7.53) [Sun] [Al] Aluminium (Z=13) abundance (Sun=6.43) [Sun] [Si] Silicium (Z=14) abundance (Sun=7.50) [Sun] [Ca] Calcium (Z=20) abundance (Sun=6.36) [Sun] [Sc] Scandium (Z=21) abundance (Sun=2.99) [Sun] [Ti] Titanium (Z=22) abundance (Sun=4.88) [Sun] [V] Vanadium (Z=23) abundance (Sun=3.91) [Sun] [Cr] Chromium (Z=24) abundance (Sun=5.61) [Sun] [Mn] Maganese (Z=25) abundance (Sun=5.47) [Sun] [Fe] Iron (Z=26) abundance (Sun=7.46) [Sun] [Co] Cobalt (Z=27) abundance (Sun=4.85) [Sun] [Ni] Nickel (Z=28) abundance (Sun=6.18) [Sun] [Sr] Strontium (Z=38) abundance (Sun=2.93) [Sun] [Y] Yttrium (Z=39) abundance (Sun=2.18) [Sun] [Zr] Zirconium (Z=40) abundance (Sun=2.46) [Sun] [Mo] Molybdene (Z=42) abundance (Sun=2.10) [Sun] [Ba] Barium (Z=56) abundance (Sun=2.18) [Sun] [La] Lanthane (Z=57) abundance (Sun=1.07) [Sun] [Ce] Cerium (Z=58) abundance (Sun=1.58) [Sun] [Nd] Neodyme (Z=60) abundance (Sun=1.40) [Sun] [Sm] Samarium (Z=62) abundance (Sun=0.88) [Sun] [Eu] Europium (Z=63) abundance (Sun=0.48) [Sun] [Fe/H] Global values for Clusters Cluster Cluster Name --- --- "[Fe/H] =" --- [Fe/H] Iron abundance of the cluster [Sun] --- "+-" --- e_[Fe/H] Mean error on [Fe/H] [Sun] Francois Ochsenbein CDS 1998 May 27 Frederic THEVENIN, Obs. Cote d'Azur Observatoire de Nice, BP 229 06304 Nice Cedex 4, France E-mail: thevenin@obs-nice.fr III_193.xml Contempory Optical Spectral Classification of the OB Stars: A Digital Atlas 3195 III/195 Atlas of Optical Spectral Classification OB Stars Contempory Optical Spectral Classification of the OB Stars: A Digital Atlas N R Walborn E L Fitzpatrick Pub. Astr. Soc. Pac. 102 379 1990 1990PASP..102..379W Stars, early-type MK spectral classification Stars, OB The Atlas provides digital spectra to assist the classification of OB spectra for 78 standard objects in the wavelength range 395.0-475.0 nm. Spectral types range from O3 - B3 (-B8 at Ia). The Atlas provides contemporary digital data comparable to the earlier printed Atlasses by Morgan et al. (1943), Abt et al. (1968), Yamashita et al. (1977) and Morgan et al. (1978). The digital data were obtained with the Shectman/Heathcote two- dimensional, photon-counting detector on the Casegrain spectrograph at the CTIO 1-meter telescope during October 1988 and March 1989. The 3-pixel resolution is 1.5 Angstroem, and the full wavelength coverage is 3800-5000 A. The data were extracted and rectified by using a uniform template followed by a low-order spine fit.
List of OB stars included in the Atlas FileName Name of FITS file in subdirectory fits --- RAh Right Ascension J2000 (hours) number=1 data added at CDS, using the SIMBAD data-base. h RAm Right Ascension J2000 (minutes) number=1 data added at CDS, using the SIMBAD data-base. min RAs Right Ascension J2000 (seconds) number=1 data added at CDS, using the SIMBAD data-base. s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) number=1 data added at CDS, using the SIMBAD data-base. deg DEm Declination J2000 (minutes) number=1 data added at CDS, using the SIMBAD data-base. arcmin DEs DEs Declination J2000 (seconds) number=1 data added at CDS, using the SIMBAD data-base. arcsec Vmag Visual magnitude number=1 data added at CDS, using the SIMBAD data-base. mag Sp Spectral Type --- LClass Luminosity Class --- alt Other name --- note a=not in the published atlas --- Paul Kuin NASA/ADC 1997 Feb 25 III_195.xml A library of near-IR stellar spectra from 1.428 to 2.5 {mu}m. 3196 III/196 Near-IR stellar spectra from 1.428 to 2.5 um A library of near-IR stellar spectra from 1.428 to 2.5 {mu}m. A Lancon B Rocca-Volmerange Astron. Astrophys. Suppl. Ser. 96 593 1992 1992A&AS...96..593L Spectra, infrared atlases stars: infrared spectroscopy stars: temperatures stars: colors This library is an EXTENDED VERSION of the library published by A.Lancon and B.Rocca-Volmerange in 1992. The catalog contains near-IR spectra of 84 stars, obtained with the Fourier Transform Spectrograph at the Canada-France-Hawaii Telescope on Mauna Kea, Hawaii. The spectra cover the H and K atmospheric windows, i.e. wavelengths from 1.43 to 2.5 microns, with a typical resolving power of 500. The spectra have all been reduced again in 1996. The general procedure was as described in the original article, except that the intrinsic energy distributions of the stars used as references were assumed to be well represented by the models of Kurucz, 1993. Making extensive use of the Simbad data base, we have searched the literature on each of these stars, looking for effective temperature and extinction determinations. The new reduction improves the reliability of the continua, and reduces possible systematic differences between observing runs. The files contain the reduced spectra in FITS format, with fluxes in arbitrary units of energy per unit frequency (normalised to approximately 1 in the K band) and frequencies in cm^-1^, the natural units of Fourier Transform spectroscopy.
List of spectra SpClass Class (dwarf, giant, supergiant) --- Object Object name --- RAh Right Ascension 2000 (hours) number=1 Position taken from SIMBAD h RAm Right Ascension 2000 (minutes) number=1 Position taken from SIMBAD min RAs Right Ascension 2000 (seconds) number=1 Position taken from SIMBAD s DE- Declination 2000 (sign) number=1 Position taken from SIMBAD --- DEd Declination 2000 (degrees) number=1 Position taken from SIMBAD deg DEm Declination 2000 (minutes) number=1 Position taken from SIMBAD arcmin DEs Declination 2000 (seconds) number=1 Position taken from SIMBAD arcsec FITSfile Name of FITS file in directory fits number=2 the full filename is concatenation of FITSfile and extension ".fit"; the corresponding file is in subdirectory fits. Spectra are normally dereddened, unless FITSname is terminated by 'r' (e.g. sp101r) which indicates a naturally reddened spectrum. --- Qual Quality of spectrum number=3 Very rough classification in 3 groups. 1=ok. 2=still ok, but not as good as 1, 3=poor (some of these would best be discarded). --- Cont Continuum model number=4 this column is empty, except if the corresponding star has been used as a reference for the correction for atmospheric absorption and for the relative flux calibration. In that case, the column indicates which Kurucz spectrum has been assumed to represent the continuum of this star. As a result of the calibration procedure, the final spectrum for a reference star will follow the Kurucz model closely (reddened, where necessary). --- H-K Color index number=5 Measured H-K (filters of Bessell and Brett, 1988PASP..100.1134B). The values are given with 3 digits, but +/- 0.015 mag. is a reasonable estimate of the 2 sigma error in general. mag (H-K)lit H-K found in the literature number=6 the H-K colour index found in the literature could be different systems. mag u_(H-K)lit Uncertainty flag on (H-K)lit --- (H-K)lit2 H-K found in the literature number=6 the H-K colour index found in the literature could be different systems. mag SpType Spectral type --- Comments Other properties found in literature --- Names Cross-identifications --- stars.tex *LaTeX tables the file should be compiled with LaTex in landscape mode; the text width could well be too big for American paper format, in this case "\small" should be changed into "\footnotesize" rawspec.fit *Raw spectrum of an O9V star this file can be used to determine in which spectral regions the quality is worst due to molecular opacity in the Earth atmosphere. Ariane Lancon Strasbourg Francois Ochsenbein CDS 1997 Feb 26 III_196.xml The Palomar/MSU nearby star spectroscopic survey. I. The northern M dwarfs-band strengths and kinematics. 3198 III/198 Palomar/MSU nearby star spectroscopic survey The Palomar/MSU nearby star spectroscopic survey. I. The northern M dwarfs-band strengths and kinematics. I N Reid S L Hawley J E Gizis Astron. J. 110 1838 1995 1995AJ....110.1838R The Palomar/MSU nearby star spectroscopic survey. I. The northern M dwarfs-band strengths and kinematics. I N Reid S L Hawley J E Gizis Astron. J. 111 2469 1996 1996AJ....111.2469R The Palomar/MSU nearby star spectroscopic survey. I. The northern M dwarfs-band strengths and kinematics. S L Hawley J E Gizis I N Reid Astron. J. 112 2799 1996 1996AJ....112.2799H The Palomar/MSU nearby star spectroscopic survey. I. The northern M dwarfs-band strengths and kinematics. S L Hawley J E Gizis I N Reid Astron. J. 113 1458 1997 1997AJ....113.1458H V/70 : CNS3 (Nearby Stars, Preliminary 3rd Version; Gliese+ 1991) Stars, nearby Stars, M-type Spectroscopy Space velocities Stars, distances The Third Catalogue of Nearby Stars (Gliese & Jahreiss, "Preliminary Version of the third Catalogue of Nearby Stars" (CNS3), 1991, catalog <V/70>) includes over 1850 stars which lie north of Dec.= -30{deg} and are either identified as spectral type M, or are unclassified but with an absolute visual magnitude estimate M_V_ > +8.0. Although there is no uniformity in selection criteria, and many of the stars lack basic data (radial velocities, spectral types, accurate photometry), the observational properties of these stars underlie most estimates of the fundamental characteristics of the Galactic Disk. We have obtained optical spectroscopy of 1746 of the 1876 stars -- the remaining 130 are binary companions of brighter stars and inaccessible to our observations. These spectra allow us, first, to exclude 61 stars as either degenerates or as misclassified earlier-type (B-K) stars lying beyond the 25 pc limit; to establish radial velocities accurate to +/-10km/s for all stars confirmed as late-type dwarfs; to determine spectral types and absolute magnitudes from the TiO bandstrength, allowing more accurate distance estimates for stars with inaccurate (or no) trigonometric parallax measurements; and to identify stars with H{alpha} emission (chromospherically active stars) and with strong CaH absorption (perhaps including some metal-poor disk subdwarfs). We have determined the nearby-star luminosity function from complete samples derived by applying both the distance limits defined by Wielen (1974, Highlights of Astron. 3, 395) and by using limits derived from our own analysis. Spectroscopic data for the southern stars (Dec.<-30{deg}) in the PMSU survey are also presented. The data were combined with the data from paper I to obtain a list of all the magnetically active dMe stars in the survey.
Basic data (tables 1a of both papers, and table 1d from paper I for Star numbers 3804-3810) Sample n=North (paper I), s=South (paper II) --- CNS3 Star number (row in CNS3) number=8 Numbers 3804 to 3810 are the additional stars from table 1d in paper I. --- Name Star name number=1 Gl - Gliese (1969, Veroff. Astr. Rechen-Instituts, Heidelberg, Nr. 22) GJ - Gliese & Jahreiss =1979A&AS...38..423G Wo - Woolley et al (1970, R. Obs. Ann., No. 5) =Cat. <V/32> LHS - Luyten Half-Second Catalogue =Cat. <I/87> LTT - Luyten Two-Tenths Catalogue LP - Luyten Palomar proper-motion catalogue G - Giclas et al (1971, Lowell Proper Motion Survey) =Cat. <I/79> GR - Giclas et al (1971) red star (see =1980LowOB...8..157G) GH - Giclas et al (1971) Hyades star (see =1962LowOB...5..257G) (Nomenclature note: should be named "HG") Rob - Robertson (should be named RBTS) =1984AJ.....89.1229R Steph - Stephenson (1986, AJ, 91, 137) =Cat. <III/123> (Nomenclature note: should be named "StKM") PS - Pesch & Sanduleak =1978AJ.....83.1090P San - Sanduleak =1976AJ.....81..350S vA - van Altena =1969AJ.....74....2V V - Vyssotsky (1963, Stars and Stellar Systems III, Basic Astronomical Data, edited by K. Aa Strand; University of Chicago Press, Chicago; p. 192) (Nomemclature Note: should be named MCC =Cat. <III/13>) --- Note1 Individual Note number=2 a Low quality trigonometric parallax b Poor photometry c Accurate parallax and good photometry. Both components of Gl 799 lie above the main-sequence. e 629 (Hy 207) appears twice in the preliminary version of the CNS3 g 2172: This star is not listed as double in the LHS h 2426 (GJ 2112 A): Eggen (1980ApJS...43..457E) notes that this star appears to be a double in good seeing, but there are no confirming observations. i 2805 (GSC036B-821) is listed in the CNS3 as a companion of V796, but the authors find that the radial velocity differs by 50km/s j star from Brosch & Goldberg (1994MNRAS.268L..27B) k star from Irwin et al. (1991MNRAS.252p..61I) --- Bin Primary or secondary binary comp. number=3 Components in a binary system are identified as p (primary) or s (secondary, tertiary). --- RAh Right ascension, 2000 h RAm Right ascension, 2000 min RAs Right ascension, 2000 s DE- Declination sign --- DEd Declination, 2000 deg DEm Declination, 2000 arcmin DEs Declination, 2000 arcsec Src Source of positional data number=4 Source of positional data: 0- P60 1- P200, Keck 2- GSC 3- CNS3 4- Digital Sky Survey Since completing the text of this paper, the authors used the on-line Digital Sky Survey to check all stars where the positions differ by more than 15 arcseconds from the CNS3 data. They assumed mean epochs of 1954.0 and 1980.0 for POSS I and UKST plates in deriving positions from the DSS. --- VMag Absolute V magnitude mag n_VMag Note about ptg/ptm origin of VMag number=5 a: CNS3 lists a photographic magnitude - the authors assumed an (m(pg)-V) colour of 1.5 magnitudes b: CNS3 lists a `photometric' magnitude for this star --- r Distance number=6 Distance and estimated uncertainty (%) from the authors' data, using a weighted combination of trigonometric and spectroscopic parallaxes. pc e_r Distance uncertainty number=6 Distance and estimated uncertainty (%) from the authors' data, using a weighted combination of trigonometric and spectroscopic parallaxes. % Dist Origin of r & M_V number=9 Origin of distance and absolute magnitude: C: distance and absolute magnitude from CNS3 S: distance estimate is based on the authors' spectroscopic data p: Distance estimate is based on trigonometric parallax --- wPi Weight for trigonometric parallax % wSp Weight for spectroscopic parallax % n_Sp Limit sign (<>) on Sp, or sd luminosity class --- Sp Spectral type --- Note3 Note about the spectrum number=7 c: Spectral type from Kirkpatrick et al (1995AJ....109..797K) d: Strong CaH - probable metal-poor disk dwarf or halo subdwarf f: 1752: Leggett & Hawkins (1988MNRAS.234.1065L) suggest, on the basis of JHK colours, that this star might be a giant, but our spectra are consistent with classification as a dwarf. Note that the V magnitude listed by LH88 is 8.07, while the CNS3 magnitude is 11.4 (photometric estimate). The authors observed a star of the latter magnitude. There is a nearby 8th magnitude SAO star (SAO 7382) - listed as K5, luminosity class unknown but mu~0arcsec/yr which Leggett & Hawkins may have observed by mistake. k: Spectral type from Kirkpatrick et al. (1995AJ....109..797K) --- Inaccessible binary companions (tables 1b) Sample n=North (paper I), s=South (paper II) --- CNS3 Star number (row number in CNS3) --- Name Star name, references same as main.dat --- Note1 Individual Note number=1 c: Gl 452B (1863) is listed as an f-type companion to Gl 452A, 7.5 magnitudes fainter and ~15 arcseconds distant. We were unable to locate this star on the TV guider (r_lim_ ~21) of the Keck telescope. d: The companion to LHS 2789 (2172) is listed in the LTT, but not in the LHS and may not exist e: Known VLM companion - Forrest et al., (1988ApJ...330L.119F) f: Eggen (1980ApJS...43..457E) noted that the primary star appeared double in good seeing, but there is no strong evidence for a binary companion. --- RAh Right ascension, 2000 h RAm Right ascension, 2000 min RAs Right ascension, 2000 s DE- Declination sign --- DEd Declination, 2000 deg DEm Declination, 2000 arcmin DEs Declination, 2000 arcsec Src Source of position, as in main.dat --- VMag Absolute V magnitude number=2 Absolute magnitudes have been calculated using the magnitudes listed in the CNS3 and the distance estimate to the primary star (either from CNS3 or main file) mag n_VMag ptg/ptm VMag estimate number=3 a: CNS3 lists a photographic magnitude b: CNS3 lists a 'photometric' magnitude estimate --- r Distance number=4 Distance and estimated uncertainty (%) from the authors' data, using a weighted combination of trigonometric and spectroscopic parallaxes. pc e_r Distance uncertainty number=4 Distance and estimated uncertainty (%) from the authors' data, using a weighted combination of trigonometric and spectroscopic parallaxes. % Vmag1 Magnitude of primary star in the system mag dV Magnitude difference mag l_dP Limit flag on dP --- dP Separation arcsec Early-type stars, giants and degenerates (tables 1c) Sample n=North (paper I), s=South (paper II) --- CNS3 Star number (row number in CNS3) --- Name Star name, references same as main.dat --- Note1 Possible error flag number=4 a: distance estimated from spectral type; b: distance estimated based on companion star; c: spectral types suggest that these stars are not associated with the nominal primary star. d: distance from CNS3 e: listed in the LHS as proper motion companion to LHS 2405 (<I/87> main file) - it is possible that we have observed the wrong star f: FS Comae - distance based on Jura & Kleinmann's (1992ApJS...83..329J) M_K g: distance from McCook & Sion (1987ApJS...65..603M) (M_V, B-V) relations --- Bin Primary or secondary binary comp. number=1 Components in a binary system are identified as p (primary) or s (secondary, tertiary). --- RAh Right ascension, 2000 h RAm Right ascension, 2000 min RAs Right ascension, 2000 s DE- Declination sign --- DEd Declination, 2000 deg DEm Declination, 2000 arcmin DEs Declination, 2000 arcsec Src Source of position, as in main.dat --- Vmag V magnitude from the CNS3 mag VMag Absolute V magnitude number=2 In North: Absolute magnitudes are derived using Reid & Murray's (1992AJ....103..514R) (M_V, (B-V)) relation unless otherwise indicated. In South: Absolute magnitudes are derived from (B-V) colours listed in the CNS3 unless otherwise indicated. mag Note2 Note about distance number=4 a: distance estimated from spectral type; b: distance estimated based on companion star; c: spectral types suggest that these stars are not associated with the nominal primary star. d: distance from CNS3 e: listed in the LHS as proper motion companion to LHS 2405 (<I/87> main file) - it is possible that we have observed the wrong star f: FS Comae - distance based on Jura & Kleinmann's (1992ApJS...83..329J) M_K g: distance from McCook & Sion (1987ApJS...65..603M) (M_V, B-V) relations --- r Distance pc Sp Spectral type --- Note3 Individual Notes number=5 d: 757: foreground reddening probably present e: Gl 288B is the well-known low-luminosity white dwarf, van Biesbroeck 3 f: Gl 432B is the well-known low-luminosity white dwarf, van Biesbroeck 4 --- Stars not observed (table 1d, paper II) CNS3 Star number (row number in CNS3) --- Name Star name --- Note1 Note flag number=1 a: Gl 127.1B probably does not exist. Gliese (1969, Veroff. Astr. Rechen-Instituts, Heidelberg, Nr. 22) lists a 'red companion at 8 arcseconds', but no companion brighter than R~17 was visible with the LCO Du Pont telescope. Bessell (1990A&AS...83..357B) lists colours of (B-V)=0.615, (V-I)=0.70, suggesting either a white dwarf companion or observations of a background star. b: Our spectrum indicates that this star is an M-dwarf, but the 6th magnitude primary, CP-73 2192, at 8 arcseconds distance prevents accurate bandstrength measurements. --- Bin Primary or secondary binary component --- RAh Right ascension, 2000 h RAm Right ascension, 2000 min RAs Right ascension, 2000 s DE- Declination sign --- DEd Declination, 2000 deg DEm Declination, 2000 arcmin DEs Declination, 2000 arcsec Src Source of position, as in main.dat --- VMag Absolute V magnitude mag r Distance pc e_r Distance uncertainty % Bandstrengths (table 3 of paper I and table 2 of paper II) Sample n=North (paper I), s=South (paper II) --- CNS3 Star number (row number in CNS3) --- m_CNS3 Multiplicity index on star --- TiO1 TiO1 index: F(6718-6723)/F(6703-6708) --- TiO2 TiO2 index: F(7058-7061)/F(7043-7046) --- TiO3 TiO3 index: F(7092-7097)/F(7079-7084) --- TiO4 TiO4 index: F(7130-7135)/F(7115-7120) --- TiO5 TiO5 index: F(7126-7135)/F(7042-7046) --- CaH1 CaH1 index: F(6380-6390)/F (6345-6355,6410-6420)) --- CaH2 CaH2 index: F(6814-6846)/F(7042-7046) --- CaH3 CaH3 index: F(6960-6990)/F(7042-7046) --- CaOH CaOH index: F(6230-6240)/F(6345-6354) --- Halpha H-alpha index: F(6560-6566)/F(6545-6555) --- Radial velocities and space motions (table 5 of paper I and table 3 of paper II) Sample n=North (paper I), s=South (paper II) --- CNS3 Star number (row number in CNS3) --- m_CNS3 Multiplicity index on star --- pmRA Proper motion in right ascension, from CNS3 arcsec/yr pmDE Proper motion in declination, from CNS3 arcsec/yr RV Radial velocity km/s Note If no proper motions are available --- U U space velocity km/s V V space velocity km/s W W space velocity km/s VMag Absolute V magnitude (from main.dat) mag Photometric and spectroscopic data for dMe stars (table 4a of paper II) CNS3 Star number (row number in CNS3) --- Halp H-alpha index: F(6560-6566)/F(6545-6555) --- TiO2 TiO2 index: F(7058-7061)/F(7043-7046) --- TiO4 TiO4 index: F(7130-7135)/F(7115-7120) --- TiO5 TiO5 index: F(7126-7135)/F(7042-7046) --- Sp Spectral type --- Mv Absolute V magnitude mag Vmag V magnitude mag R-I R-I colour index mag V-I V-I colour index mag r_VRI Reference for VRI photometry --- V-K V-K colour index mag S(Hb) H{beta} flux 10-13mW/m2 S(Ha)/S(Hb) H{alpha} versus H{beta} flux ratio --- log(L(Ha)/Lbol) H{alpha} vs. bolometric luminosity ratio --- Mbol Bolometric magnitude mag Photometric and spectroscopic data for Hyades stars (table 4b of paper II) Photometric and spectroscopic data for IC 2602 stars (table 4c of paper II) CNS3 Star number (row number in CNS3) --- Halp H-alpha index: F(6560-6566)/F(6545-6555) --- TiO2 TiO2 index: F(7058-7061)/F(7043-7046) --- TiO4 TiO4 index: F(7130-7135)/F(7115-7120) --- TiO5 TiO5 index: F(7126-7135)/F(7042-7046) --- Sp Spectral type --- Mv Absolute V magnitude mag Vmag V magnitude mag V-I V-I colour index mag log(L(Ha)/Lbol) H{alpha} versus bolometric luminosity ratio --- log(LX/Lbol) X-ray versus bolometric luminosity ratio --- Mbol Bolometric magnitude mag paper1.tex Tables from paper I, latex paper2.tex Tables from paper II, latex Francois Ochsenbein CDS 1997 May 14 It is a pleasure to thank Suzanne Hawley <slh@pillan.pa.msu.edu>, who kindly provided a latex version of the tables. III_198.xml The Observed Periods of Ap and Bp stars 3199A III/199A Observed Periods of Ap and Bp stars The Observed Periods of Ap and Bp stars F A Catalano P Renson Astron. Astrophys. Suppl. Ser. 127 421 1998 1998A&AS..127..421C III/162 : General Catalogue of Ap and Am stars (Renson+ 1991) Aitken R.G., 1932, New General Catalogue of Double Stars. Publ. Carnegie Inst. Washington No.417 Babcock H.W., 1947ApJ...105..105B Babcock H.W., 1957ApJS....3..141B Batten A.H., Fletcher J.M., Mann P.J., 1978PDAO...15..121B Boss B., 1937, General Catalogue of 33342 Stars , Cat. <I/113> Catalano F.A., Renson P., 1984A&AS...55..371C, Cat. <III/152> Catalano F.A., Renson P., 1988A&AS...72....1C Catalano F.A., Renson P., Leone F., 1991A&AS...87...59C Catalano F.A., Renson P., Leone F., 1993A&AS...98..269C Catalano F.A., Renson P., 1997A&AS..121...57C Morgan W.W., 1931a, 1931ApJ....73..104M Morgan W.W., 1931b, 1931ApJ....74...24M Morgan W.W., 1932ApJ....75...46M Morgan W.W., 1933a, 1933ApJ....77...77M Morgan W.W., 1933b, 1933ApJ....77..330M Preston G.W., 1974ARA&A..12..257P Renson P., Gerbaldi M., Catalano F.A., 1991A&AS...89..429R, Cat. <III/162> Stars, Ap Stars, Bp Stars, variable catalogs stars: chemically peculiar stars: variable: other A catalogue of all the periods published up to 31 October 1996 on 364 CP stars is presented; it supersedes the previous version (catalog <III/152>). The paper version (catalog.tex) is arranged in three tables: the bulk of the data, i.e. those referring to CP2, CP3, and CP4 stars, are given in Table 1, while the data concerning He-strong stars are given in Table 2 and those for eclipsing or ellipsoidal variables are collected in Table 3. Notes are also provided at the end of each table, mainly about duplicities. The machine-readable version was arranged in two main parts: the main parameters of the 364 stars (identifiers and names, positions, spectral types, magnitudes and peculiarities) are tabulated in the file 'stars'; periods and the of the observed variations (light, spectrum, magnetic field, etc.) are listed in the 'periods' file. Two other files contains the notes and the references.
List of the CP stars Star Star name (HD or Rns) --- Table Table number number=1 In the paper, Table 1 deals with CP2, CP3 and CP4 stars; Table 2 deals with He-string stars, and Table 3 with eclipsing or ellipsoidal variables. --- HD HD (Cat. <III/135>) number --- m_HD Multiplicity index on HD --- HR HR (Cat. <V/50>) number --- m_HR Multiplicity index on HR --- Rns Renson (Cat. <III/162>) number --- Name Star name --- VarName Variable name --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec SpType Spectral type number=2 He wk means that the star belongs the the He weak subgroup. --- Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag --- l_Per 'Approximative' flag on Per --- Per Main Period d n_Per2 + when two periods exist --- Per2 Second period (HD 25267 only) d u_Per Uncertainty flag on Per number=3 : approximate value ? dubious value --- n_Per l: long. --- Var type of variability number=4 l: luminosity and/or color m: magnetic field s: spectral line intensity v: wavelength displacements of the lines of an ion, interpreted as mean radial velocity variations for that ion. --- Note indicates a remark in notes.dat file --- List of Period values and variability types Star Star name, as in file 'stars' --- Table Table number, as in file 'stars' --- Part Catalogue part number=1 0: main catalogue, Catalano & Renson, 1984, Cat. <III/152> 1: first supplement, Catalano & Renson, 1988A&AS...72....1C 2: second supplement, Catalano et al., 1991A&AS...87...59C 3: third supplement, Catalano et al., 1993A&AS...98..269C 4: fourth supplement, Catalano & Renson, 1997A&AS..121...57C blank: new reference or old reference only now added --- l_Per Limit flag on Per --- Per Period (in days except when x_Per=y or m) d u_Per Uncertainty flag on Per number=2 : approximate value ? dubious value ) less probable value --- x_Per y when the period is expressed in years m when the period is expressed in months --- e_Per rms uncertainty on Per d Perl Lower limit for period when interval d --- Separation dash --- Peru upper limit for period when interval d u_Perl Uncertainty flag on Perl number=2 : approximate value ? dubious value ) less probable value --- x_Peru y when the period is expressed in years --- Rem Remarks number=3 onb: or other nearby values ov: or other values ct: constant nv: no variability v?: variable? np: no period l)?: long)? l?: long? --- Note Notes number=4 Individual Notes: HD 18296 : 2.88422 (+ 40 to 50 years ?) HD 25267 : 3.84394 +1.21005 l Manfroid et al. 1985 1.21005 +3.83394 l(IR) Catalano et al. 1991 HD 32549 : (prob. 4.6398+/-0.0008) HD 37151 : 5.6732+/-0.0143+4.1513+/-0.0092? l North 1984 HD 112185 : 1.14229 v + 8.0... s,v + long HD 89822 : no var with P=7.56 HD 94660 : no var. during 8 d l (Heck et al. 1976) HD 94660 : no var. during 9 d l (Renson & Manfroid 1978a) HD 123515 : 1.45594 + 1.5168 + 1.3725 + 2.1818 l Waelkens 1993 HD 144334 : 3.61+0.04-0.06 m Borra et al. 1983 HD 152107A: 3.85646 (+12.5 years) m, v Gerth 1990 HD 176232 : ampl. 0.01:, short time scale l Hube & Anderson 1986 HD 196502 : 20.2754 s, m + 551 v Preston 1967 HD 201433A: 1.12912 + 1.19328 l Guthnik 1942 HD 219749 : 1.618 s + 48.304 v(SB) Hube 1979 HD 224801 : 3.7397 l + 4.8833 v Rakosch 1963a HD 38602 : (+irreg.) l Groenbech & Naqvi 1976 --- Var Type of variability --- Ref References --- Individual notes to flagged stars Star Star name, as in file 'stars' --- Cont Continuation letter --- Text Text of Reference --- catalog.tex LaTeX version of the catalog Patricia Bauer, Francois Ochsenbein CDS 1997 Nov 21 Is is a pleasure to thank Dr Francesco Catalano (email: FCATALANO@alpha4.ct.astro.it), who kindly prepared this new version of the Catalog of the Periods of Ap and Am stars in February 1997 on request from CDS. UNKNOWN UNKNOWN This version of the catalog, superseding the one distributed by CDS between July 1997 and February 1998, differs for only 7 stars. III_199A.xml A Catalogue of [Fe/H] determinations : 1996 Edition 3200A III/200A Catalogue of [Fe/H] A Catalogue of [Fe/H] determinations : 1996 Edition G Cayrel de Strobel C Soubiran E D Friel N Ralite P Francois Astron. Astrophys. Suppl. Ser. 124 299 1997 1997A&AS..124..299C Abundances Abundances, [Fe/H] Effective temperatures catalogs stars: abundances stars: atmospheres stars: fundamental parameters The catalogue includes [Fe/H] determinations and atmospheric parameters (Teff, logg ) obtained from high resolution spectroscopic observations and detailed analyses, most of them carried out with the help of model-atmospheres. This fifth Edition of the catalogue contains 5946 determinations for 3247 stars, including 751 stars in 84 associations, clusters or galaxies. The literature (700 bibliographical references) is complete up to December 1995. The Catalogue is made up of three tables : Table 1 : field stars Table 2 : stars in galactic associations and clusters, and in SMC, LMC, M33 Table 3 : numbered list of bibliographical references
Spectroscopic [Fe/H] for field stars (table 1) ID Designation (SIMBAD name) --- SpType Spectral type --- Type Object type number=1 Object type : cf SIMBAD user's guide and reference manual, appendix F --- Vmag V visual magnitude mag B-V B-V colour index mag flag1 Photometric flag number=2 D : joint magnitude in binary stars V : variable magnitude : : large uncertainty in photometry --- Teff Effective temperature K logg Logarithm of gravity [cm/s2] [Fe/H] Abundance Sun flag2 Spectroscopic flag number=3 S : result from a spectrum of low signal to noise ratio M : average of several values given in the corresponding article C : in the absence of any indication in the corresponding article, [Fe/H] relative to the Sun was calculated with a solar value of 7.50 T : M + C D : S + C --- stand Comparison star from which [Fe/H] was obtained --- Nref Number of the reference detailed in refs.dat --- Spectroscopic [Fe/H] for other stars (table 2) Cluster Cluster name number=1 NGC 1977 = NGC 1977 and Orion Association --- ID Designation (SIMBAD name) --- SpType Spectral type --- Type Object type number=2 Object type : cf SIMBAD user's guide and reference manual, appendix F --- Vmag V visual magnitude mag B-V B-V colour index mag flag1 Photometric flag number=3 D : joint magnitude in binary stars V : variable magnitude : : large uncertainty in photometry --- Teff Effective temperature K logg Logarithm of gravity [cm/s2] [Fe/H] Abundance Sun flag2 Spectroscopic flag number=4 S : result from a spectrum of low signal to noise ratio M : average of several values given in the corresponding article C : in the absence of any indication in the corresponding article, [Fe/H] relative to the Sun was calculated with a solar value of 7.50 T : M + C D : S + C --- stand Comparison star from which [Fe/H] was obtained --- Nref Number of the reference detailed in refs.dat --- Numbered bibliographical references (table 3) Nref Number of the reference (chronological order) --- RefText Full reference --- C. Soubiran, Observatoire de Bordeaux 1996 Nov 26 Caroline Soubiran <Caroline.Soubiran@observ.u-bordeaux.fr> UNKNOWN UNKNOWN * 26-Nov-1996: first version * 10-Mar-1998: version 'A', incorporates corrections in table fistars.dat (table1) communicated by Caroline Soubiran. * This catalogue supersedes the 1991 version <III/165> (1992A&AS...95..273C) III_200A.xml The Pulkovo spectrophotometric catalog of bright stars in the range from 320 to 1080nm 3201 III/201 Pulkovo Spectrophotometric Catalog The Pulkovo spectrophotometric catalog of bright stars in the range from 320 to 1080nm G A Alekseeva A A Arkharov V D Galkin E I Hagen-Thorn I N Nikanorova V V Novikov V B Novopashenny V P Pakhomov E V Ruban D E Shchegolev Baltic Astron. 5 603 1996 1996BaltA...5..603A The Pulkovo spectrophotometric catalog of bright stars in the range from 320 to 1080nm G A Alekseeva A A Arkharov V D Galkin E I Hagen-Thorn I N Nikanorova V V Novikov V B Novopashenny V P Pakhomov E V Ruban D E Shchegolev Baltic Astron. 6 481 1997 1997BaltA...6..481A II/85 : Absolute Calibration of Stellar Spectrophotometry (Johnson 1980) III/202 : Spectrophotometric Catalogue of Stars (Kharitonov+, 1988) Spectrophotometry Stars, bright A complete list of the observed stars is given in Table 4. The following information about the stars is given: HR and HD numbers, the Bayer's name, the number of independent scans of the spectrum (short-/long-wavelength range), equatorial coordinates for 2000.0, spectral type from the 1982 version of the BS catalog, magnitude V and color index B-V from the same source. Information on binarity and variability is given in the remarks following Table 4. For the visual binaries, the separation and m are taken also from the BS . For the variables, variability type and magnitudes at the maximum and minimum light and the period are from the General Catalog of Variable Stars (Kholopov et al. 1985-1990) and its three Supplements (Inf. Bull. Var. Stars Nos. 2681, 3058, and 3323). The final energy distribution data in the range 320-1080 nm with a step 2.5 nm, expressed in W/m2/m (or 10^-6^arg/cm^2^/s/nm in cgs) given in Tables 5, 5a and 6. Tables 5 contains the combined data covering the wavelengths 320-1080 nm and Table 5a is for the stars having data only in the 500-1080 nm range. All the data are for the same effective spectral broadening, 10 nm. The data covering only the wavelengths 320-735 nm (with effective spectral broadening of 5 nm) are presented in Table 6. A spectrophotometric catalog is presented, combining results of numerous observations by Pulkovo astronomers at different observing sites. The catalog consists of three parts: the first contains the data of 602 stars in the spectral range 320-735 nm with a resolution 5 nm; the second one contains 285 stars in the spectral range of 500-1080 nm with resolution10 nm and the third one contains 278 stars combined from the preceding catalogs in spectral range 320-1080 nm with resolution 10 nm. The data are presented in the absolute energy units W/mm, with step of 2.5 nm and with an accuracy no more than 1.5 - 2.0%.
List of stars (table4 of paper I) HR Designation of the star in the Bright Star Catalog <V/50> --- m_HR Multiplicity --- HD Designation in the Hentry Draper Catalog <III/135> --- Name Star name --- Ns(short) Number of scans (short wavelength) --- Ns(long) Number of scans (long wavelength) --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin SpType MK Spectral Classification --- Vmag V magnitude mag B-V color index mag table Table containing the spectrophotometry the spectrophotometry is in tables: 5 : spectrophotometry in table5.dat (range 320-1080nm) 6 : spectrophotometry in table6.dat (range 500-1080nm) a : spectrophotometry in table5a.dat (range 320-735nm) b : spectrophotometry in both table5.dat and table6.dat --- Note note detailed in file notes.dat --- Notes to stars.dat HR Designation of the star as in table4.dat --- m_HR Multiplicity --- about Note about Variability or Duplicity --- --- Colon --- Text Text of note the following abbreviations are used: ExtSt = Standard for definitions of atmospheric extinction. NSV = number from "New Catalogue of Suspected Variable Stars" (catalog <II/140>, 1982) PSt = Primary standard; SSt = Secondary standard; TSt = Tertiary standard; --- Francois Ochsenbein CDS 1997 Sep 30 It is a pleasure to thank Dr Victor Novikov <novikov@pulobs.spb.su> Pulkovo Observatory, St. Petersburg, Russia who provided the data to CDS in September 1997. III_201.xml Spectrophotometric Catalogue of Stars 3202 III/202 Spectrophotometric Catalogue of Stars Spectrophotometric Catalogue of Stars A V Kharitonov V M Tereshchenko L N Knyazeva Alma-Ata, Nauka, p. 484 ??? ??? 1988 1988scs..book.....K Spectrophotometry Energy distributions This catalogue contains the absolute energy distribution of the 1147 stars of different spectral type and luminosity classes in the range of 3225-7575A with the step 50A. The observations were made in the Fessenkov Astrophysical Institute (AlmaAta,Kazakstan, height 1450m) during 1968-1986 using spectrum scanner with photo-multiplier tube attached to the 50cm Cassegrain telescope. Standards are Beta Ari, Gamma Ori, Beta Tau, Alpha Leo, Eta UMa, Alpha Lyr, Alpha Aql and Alpha Peg, based on the absolute energy distribution of Vega as given Hayes(1985). The average accuracy of the catalogue data is 3.5%.
Energy distribution (W/(m2.m)) No Running number --- RAh Right Ascension 2000 (hours) number=1 the positions were not present in the original catalog; they were taken from SIMBAD h RAm Right Ascension 2000 (minutes) number=1 the positions were not present in the original catalog; they were taken from SIMBAD min RAs Right Ascension 2000 (seconds) number=1 the positions were not present in the original catalog; they were taken from SIMBAD s DE- Declination 2000 (sign) number=1 the positions were not present in the original catalog; they were taken from SIMBAD --- DEd Declination 2000 (degrees) number=1 the positions were not present in the original catalog; they were taken from SIMBAD deg DEm Declination 2000 (minutes) number=1 the positions were not present in the original catalog; they were taken from SIMBAD arcmin DEs Declination 2000 (seconds) number=1 the positions were not present in the original catalog; they were taken from SIMBAD arcsec HR Name in Bright Star catalogue --- HD Name in HD catalogue --- Vmag Magnitude mag Sp Spectral type --- E3225 Flux in wavelength 3225A 0.1uW/m2/m E3275 Flux in wavelength 3275A 0.1uW/m2/m E3325 Flux in wavelength 3325A 0.1uW/m2/m E3375 Flux in wavelength 3375A 0.1uW/m2/m E3425 Flux in wavelength 3425A 0.1uW/m2/m E3475 Flux in wavelength 3475A 0.1uW/m2/m E3525 Flux in wavelength 3525A 0.1uW/m2/m E3575 Flux in wavelength 3575A 0.1uW/m2/m E3625 Flux in wavelength 3625A 0.1uW/m2/m E3675 Flux in wavelength 3675A 0.1uW/m2/m E3725 Flux in wavelength 3725A 0.1uW/m2/m E3775 Flux in wavelength 3775A 0.1uW/m2/m E3825 Flux in wavelength 3825A 0.1uW/m2/m E3875 Flux in wavelength 3875A 0.1uW/m2/m E3925 Flux in wavelength 3925A 0.1uW/m2/m E3975 Flux in wavelength 3975A 0.1uW/m2/m E4025 Flux in wavelength 4025A 0.1uW/m2/m E4075 Flux in wavelength 4075A 0.1uW/m2/m E4125 Flux in wavelength 4125A 0.1uW/m2/m E4175 Flux in wavelength 4175A 0.1uW/m2/m E4225 Flux in wavelength 4225A 0.1uW/m2/m E4275 Flux in wavelength 4275A 0.1uW/m2/m E4325 Flux in wavelength 4325A 0.1uW/m2/m E4375 Flux in wavelength 4375A 0.1uW/m2/m E4425 Flux in wavelength 4425A 0.1uW/m2/m E4475 Flux in wavelength 4475A 0.1uW/m2/m E4525 Flux in wavelength 4525A 0.1uW/m2/m E4575 Flux in wavelength 4575A 0.1uW/m2/m E4625 Flux in wavelength 4625A 0.1uW/m2/m E4675 Flux in wavelength 4675A 0.1uW/m2/m E4725 Flux in wavelength 4725A 0.1uW/m2/m E4775 Flux in wavelength 4775A 0.1uW/m2/m E4825 Flux in wavelength 4825A 0.1uW/m2/m E4875 Flux in wavelength 4875A 0.1uW/m2/m E4925 Flux in wavelength 4925A 0.1uW/m2/m E4975 Flux in wavelength 4975A 0.1uW/m2/m E5025 Flux in wavelength 5025A 0.1uW/m2/m E5075 Flux in wavelength 5075A 0.1uW/m2/m E5125 Flux in wavelength 5125A 0.1uW/m2/m E5175 Flux in wavelength 5175A 0.1uW/m2/m E5225 Flux in wavelength 5225A 0.1uW/m2/m E5275 Flux in wavelength 5275A 0.1uW/m2/m E5325 Flux in wavelength 5325A 0.1uW/m2/m E5375 Flux in wavelength 5375A 0.1uW/m2/m E5425 Flux in wavelength 5425A 0.1uW/m2/m E5475 Flux in wavelength 5475A 0.1uW/m2/m E5525 Flux in wavelength 5525A 0.1uW/m2/m E5575 Flux in wavelength 5575A 0.1uW/m2/m E5625 Flux in wavelength 5625A 0.1uW/m2/m E5675 Flux in wavelength 5675A 0.1uW/m2/m E5725 Flux in wavelength 5725A 0.1uW/m2/m E5775 Flux in wavelength 5775A 0.1uW/m2/m E5825 Flux in wavelength 5825A 0.1uW/m2/m E5875 Flux in wavelength 5875A 0.1uW/m2/m E5925 Flux in wavelength 5925A 0.1uW/m2/m E5975 Flux in wavelength 5975A 0.1uW/m2/m E6025 Flux in wavelength 6025A 0.1uW/m2/m E6075 Flux in wavelength 6075A 0.1uW/m2/m E6125 Flux in wavelength 6125A 0.1uW/m2/m E6175 Flux in wavelength 6175A 0.1uW/m2/m E6225 Flux in wavelength 6225A 0.1uW/m2/m E6275 Flux in wavelength 6275A 0.1uW/m2/m E6325 Flux in wavelength 6325A 0.1uW/m2/m E6375 Flux in wavelength 6375A 0.1uW/m2/m E6425 Flux in wavelength 6425A 0.1uW/m2/m E6475 Flux in wavelength 6475A 0.1uW/m2/m E6525 Flux in wavelength 6525A 0.1uW/m2/m E6575 Flux in wavelength 6575A 0.1uW/m2/m E6625 Flux in wavelength 6625A 0.1uW/m2/m E6675 Flux in wavelength 6675A 0.1uW/m2/m E6725 Flux in wavelength 6725A 0.1uW/m2/m E6775 Flux in wavelength 6775A 0.1uW/m2/m E6825 Flux in wavelength 6825A 0.1uW/m2/m E6875 Flux in wavelength 6875A 0.1uW/m2/m E6925 Flux in wavelength 6925A 0.1uW/m2/m E6975 Flux in wavelength 6975A 0.1uW/m2/m E7025 Flux in wavelength 7025A 0.1uW/m2/m E7075 Flux in wavelength 7075A 0.1uW/m2/m E7125 Flux in wavelength 7125A 0.1uW/m2/m E7175 Flux in wavelength 7175A 0.1uW/m2/m E7225 Flux in wavelength 7225A 0.1uW/m2/m E7275 Flux in wavelength 7275A 0.1uW/m2/m E7325 Flux in wavelength 7325A 0.1uW/m2/m E7375 Flux in wavelength 7375A 0.1uW/m2/m E7425 Flux in wavelength 7475A 0.1uW/m2/m E7475 Flux in wavelength 7475A 0.1uW/m2/m E7525 Flux in wavelength 7525A 0.1uW/m2/m E7575 Flux in wavelength 7575A 0.1uW/m2/m V.S.Avedisova Moscow 1997 Mar 26 III_202.xml Catalogue of stars in the Northern Milky Way having H-{alpha} in emission 3205 III/205 H-alpha Stars in Northern Milky Way Catalogue of stars in the Northern Milky Way having H-{alpha} in emission L Kohoutek R Wehmeyer Abhandlungen Hamburger Sternwarte 11, Teil 1 + 2 ??? ??? 1997 1997AAHam..11....1K http://www.hs.uni-hamburg.de/german/persons/kohoutek.html : Charts Stars, emission Milky Way Cross identifications The catalogue contains 4174 stars in the Northern Milky Way, in the range 32{deg}<l<214{deg}, -10{deg}<b<+10{deg}, having the H line in emission. The HBH list (main list, Schmidt camera Hamburg-Bergedorf, red plates taken in the years 1964-70) contains 1979 objects partly identical with those in other lists of H emission-line stars given in the literature up till 1994. Non-stellar objects (e.g. HII regions, planetary nebulae) have not been included in this catalogue except for those objects containing central stars which have the H line in emission, and also for some doubtful cases. Copyright: 1997 by Hamburger Sternwarte (ISSN 0374-1583)
The Catalogue ID Designation of the star The number if made from the page header (1 to 70) and a running number on the page (1 to 60). --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg n_Vmag Magnitude system colour system given in the literature: (blank) photoelectric in the V system, B photoelectric in the B system, v visual or photovisual, p photographic, r red or photored, m spectral region not known, e estimated on our Schmidt-camera plates (A10) according to the classification of the spectra of HBH stars (see Section 2) --- Vmag Magnitude in V, or see n_Vmag V following the magnitude means variable star; the given brightness corresponds to that of the maximum. We confirmed the variability of many stars and found several new variable stars. mag u_Vmag Magnitude variability or uncertainty --- SpType Spectral type given in the literature --- n_SpType indicates a remark --- POSS POSS O-chart on which x and y are measured The 6-digit number represents the Declination in degrees, followed by the Right Ascension in hours and minutes, of the center; for instance, 600000 means +60{deg}, 00h00m POSS plate. --- xPOSS Position on O plate from left inner edge mm yPOSS Position on O plate from lower inner edge mm HBH Hamburg-Bergedorg star having H-alpha in em. S (at the end, but not part of the designation) indicates an object having a suspected H{alpha} emission line or perhaps a non-stellar object. There are two reasons for a designation as ``suspected'': a) the contrast between the H{alpha} emission line and the continuum in the neighbourhood is small, b) the object may not be a stellar one: e.g. the object is a compact HII region, a knot of the large HII region or a planetary nebula --- SC Classification of Spectrum Classification of the spectrum of HBH stars on the Schmidt camera long-exposed (30 min) red plates. -> H{alpha} emission line is (first character): 1 = very faint, 2 = faint, 3 = moderate, 4 = strong, 5 = overexposed; -> continuum is (second character): - = invisible or very faint, A = faint, B = moderate, C = strong, D = overexposed, -- is found when no classification of the spectrum in the above system possible, mainly because H emission line visible on short-exposed (<30 min) plates only, or because of variability; --- FC Existence of finding charts Existence of the finding chart in Part 2: 1 = one chart, 2 = two charts. See the range of RA given on Plates. --- HD HD or HDE number --- u_HD Uncertainty flag on HD identification --- Name Star (variable) name --- BD Bonner Durchmusterung designation --- MWC Designation in Mount Wilson Catalog or Additional Stars (AS) --- u_MWC Uncertainty flag on MWC identification --- LS Designation in "Luminous Stars in Northern Milky Way" (cat. <III/76>) --- Bidelman Number in Bidelman (1954ApJS....1..175B) --- He3 Number in Henize (1976ApJS...30..491H) --- Ton Designation in Tonantzintla lists --- VES Designation in Vatican catalogue (1977-83) --- Other Designation in further 91 lists --- Rem when a note exists in file notes.dat --- Remarks to individual stars ID Designation of the star, as in catalog --- Text Text of remark --- hac-ta.tex LaTeX Catalog, A pages 1-70 hac-tb.tex LaTeX Catalog, B pages 1-70 hac-tc.tex LaTeX Catalog, C pages 71-94 hac-tit.tex title pages of Part 1 and Part 2 hac-txt.ps text (pages 1-24 without figure), PostScript hac-txt.tex text (pages 1-24 without figure), LaTeX Francois Ochsenbein CDS 1998 May 05 It is a pleasure to thank Prof. Lubos Kohoutek who kindly supplied a copy of the catalogue, on paper and on diskette, to CDS (Francois Ochsenbein) in April 1998 III_205.xml MK spectral classifications, 13th General Catalogue, Epoch 2000, including UBV photometry 3206 III/206 13th General Catalogue of MK Spectral Classification MK spectral classifications, 13th General Catalogue, Epoch 2000, including UBV photometry W Buscombe Northwestern Univ., Evanston, Illinois ISBN 0-939160-11-3 ??? ??? 1998 Spectral types Photometry, UBV A file of MK spectral types and UBV photometry maintained at Dearborn Observatory is presented here. It is based on an extensive literature search. The annex files (various clusters and associations, and SMC) are from the revised 12th catalogue.
The 13th General Catalogue Data for IC1805 Data for NGC 752 Data for Orion trapezium Data for NGC 3293 Data for NGC 6087 Data for NGC 6475 (M 7) Data for Orion association Data for upper Sco and Oph association Data for Small Magellanic Cloud Id Identification for star --- RAh Right Ascension (2000) hour h RAm Right Ascension (2000) minute the columns RAm and DEd are blank only for a few stars in files ngc1977.dat and ngc6087.dat min DE- Declination sign --- DEd Declination (2000) degree deg DEm Declination (2000) minute arcmin u_DEm DEm uncertain --- SpType MK type --- n_SpType '*' for a standard --- n_Vmag 'B' when Vmag represents a B magnitude --- Vmag Johnson V magnitude mag u_Vmag Uncertainty or mean flag on Vmag The letter 'm' (for mean) is used for mean magnitude of variables (the magnitude is printed within angle brackets like <14.8>) --- B-V Johnson B-V color mag u_B-V mean flag on B-V --- U-B Johnson U-B color mag Name Alternate identification, usually HD --- Francois Ochsenbein CDS 1998 Dec 10 William Buscombe, Derborn Observatory <buscombe@nwu.edu> III_206.xml Moscow Spectrophotometric Catalog of Stars 3207 III/207 Moscow Spectrophotometric Catalog Moscow Spectrophotometric Catalog of Stars I N Glushneva V T Doroshenko T S Fetisova T S Khruzina E A Kolotilov L V Mossakovskaya V I Shenavrin I B Voloshina V V Biryukov L S Shenavrina Soobshch. Gos. Astron. Inst. P.K. Shternberga 219 3 1980 1980SoSht.219....3K Moscow Spectrophotometric Catalog of Stars I N Glushneva V T Doroshenko T S Fetisova T S Khruzina E A Kolotilov L V Mossakovskaya V I Shenavrin I B Voloshina V V Biryukov L S Shenavrina Astron. Zh. 57 1003 1980 1980AZh....57.1003V Moscow Spectrophotometric Catalog of Stars I N Glushneva V T Doroshenko T S Fetisova T S Khruzina E A Kolotilov L V Mossakovskaya V I Shenavrin I B Voloshina V V Biryukov L S Shenavrina Trudy Gosud. Astron. Inst. Shternberga 52 182 1982 1982TrSht..52..182V Moscow Spectrophotometric Catalog of Stars I N Glushneva V T Doroshenko T S Fetisova T S Khruzina E A Kolotilov L V Mossakovskaya V I Shenavrin I B Voloshina V V Biryukov L S Shenavrina Trudy Gosud. Astron. Inst. Shternberga 55 84 1983 1983TrSht..55...84V Moscow Spectrophotometric Catalog of Stars I N Glushneva V T Doroshenko T S Fetisova T S Khruzina E A Kolotilov L V Mossakovskaya V I Shenavrin I B Voloshina V V Biryukov L S Shenavrina Trudy Gosud. Astron. Inst. Shternberga 61 272 1989 1989TrSht..61..272S Moscow Spectrophotometric Catalog of Stars I N Glushneva V T Doroshenko T S Fetisova T S Khruzina E A Kolotilov L V Mossakovskaya V I Shenavrin I B Voloshina V V Biryukov L S Shenavrina Trudy Gosud. Astron. Inst. Shternberga 62 119 1991 1991TrSht..62..119S III/126 : Stellar Spectrophotometric Catalogue (Burnashev, 1985) III/202 : Spectrophotometric Catalogue of Stars (Kharitonov+, 1988) III/208 : Sternberg Spectrophotometric Catalog (Glushneva+ 1998) III/209 : Spectrophotometric Standards (Biryukov+ 1998) J/A+AS/92/1 : Secondary Spectrophotometric standards (Glushneva+ 1992) Spectrophotometry Energy distributions stars: energy distribution stars: near-infrared This catalogue contains the energy distribution of 223 stars of different spectral type and luminosity classes in the range 5975-10825{AA} with the step 50A. The observations were made at the Crimean Station of the Sternberg Astronomical Institute during 1978-1990 using near-infrared spectrophotometer installed at the 48-cm and 60-cm Zeiss reflectors. Standards are {beta} Ari, {gamma} Ori, {beta} Tau, {alpha} Leo, {eta} UMa, {alpha} Lyr, {alpha} Aql and {alpha} Peg. Energy distribution data in the spectra of standard stars was taken according to Volosina, Glushneva and Shenavrin (1980AZh....57.1003V). Monochromatic fluxes are in erg/(cm^2^.s.cm). Zero flux is expressed as 0.E+00.
Energy distribution of 223 stars in the range 5975-10825{AA} in erg/(cm^2^.s.cm) Seq Running number --- HR Name in Bright Star catalogue (Cat. <V/50>) --- HD Name in HD catalogue (Cat. <III/135>) --- Name Name of star --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign (2000.0) --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin Vmag V magnitude mag B-V B-V color index mag U-B U-B color index mag SpType Spectral type and luminosity class --- Nobs Number of observation in different night --- E Energy distribution data in erg/(cm^2^.s.cm) with the step 50{AA} in the range 5975-10825{AA} mW/m2/cm Veta Avedisova INASAN 1998 Dec 18 III_207.xml Spectrophotometric Standards of 7-8 mag 3209 III/209 Spectrophotometric Standards Spectrophotometric Standards of 7-8 mag V V Biryukov G V Borisov I N Glushneva V I Shenavrin Astron. Astrophys. Transact., 16, No1 ??? ??? 1998 Spectrophotometric Standards of 7-8 mag V V Biryukov G V Borisov I N Glushneva V I Shenavrin Astron. Astrophys. Transact., ??? ??? in press III/126 : Stellar Spectrophotometric Catalogue (Burnashev, 1985) III/202 : Spectrophotometric Catalogue of Stars (Kharitonov+, 1988) III/207 : Moscow Spectrophotometric Catalog (Glushneva+ 1998) III/208 : Sternberg Spectrophotometric Catalog (Glushneva+ 1998) J/A+AS/92/1 : Secondary Spectrophotometric standards (Glushneva+ 1992) Spectrophotometry Energy distributions Stars, standard energy distribution photometry standards The catalog contains energy distribution data of 82 stars of 7-8mag belonging to spectral types A0-G2. Spectral energy distribution is presented in the range 3400-7500{AA} with 50{AA} step. The observations were made in the period 1991-1996 by means of the spectrophotometer working at the regime of the photon counting. Scanner was installed at the 60-cm Zeiss reflector of the Sternberg Institute Crimean Station. Eight early type stars were used as spectrophotometic standards: {beta} Ari, {gamma} Ori, {beta} Tau, {alpha} Leo, {eta} UMa, {alpha} Lyr, {alpha} Aql and {alpha} Peg. The accuracy of the monochromatic fluxes is about 2% in the ultraviolet, 1% in the visual range an 1.5-2% for {lambda}>7000{AA}. The energy distribution data are expressed in erg/(cm^2^.s.cm)*10^-6^.
Star summary (SIMBAD data) Seq Running number --- HD HD number of the star --- RAh Right Ascension J2000 (hours) number=1 Data are from SIMBAD h RAm Right Ascension J2000 (minutes) number=1 Data are from SIMBAD min RAs Right Ascension J2000 (seconds) number=1 Data are from SIMBAD s DE- Declination J2000 (sign) number=1 Data are from SIMBAD --- DEd Declination J2000 (degrees) number=1 Data are from SIMBAD deg DEm Declination J2000 (minutes) number=1 Data are from SIMBAD arcmin DEs Declination J2000 (seconds) number=1 Data are from SIMBAD arcsec Bmag Blue magnitude number=1 Data are from SIMBAD mag Vmag Visual magnitude number=1 Data are from SIMBAD mag SpType Spectral type number=1 Data are from SIMBAD --- Energy distribution of 82 stars in the range 3425-7525{AA} in erg/(cm^2^.s.cm)*10^-06^ Seq Running number --- Name Star Name, in HD catalogue (Cat. <III/135>) --- E Energy distribution data in 10^-06^(erg/cm2.s.cm) with the step 50{AA} in the range 3425-7525{AA} nW/m2/cm Veta Avedisova INASAN 1998 Dec 18 III_209.xml A Catalogue of Spectroscopically Identified White Dwarfs (4th edition, V.2) 3210 III/210 Spectroscopically Identified White Dwarfs A Catalogue of Spectroscopically Identified White Dwarfs (4th edition, V.2) G P McCook E M Sion Astrophys. J. Suppl. Ser. 121 1 1999 1999ApJS..121....1M Stars, white dwarf A catalog of 2249 white dwarfs which have been identified spectroscopically is presented complete through 1996 April. This compilation is the fourth edition of the Villanova Catalog of Spectroscopically Identified White Dwarfs. For each degenerate star, the following data entries with references are provided: (1) catalog coordinate designation or WD number, in order of right ascension; (2) the right ascension and declination for epoch 1950.0; (3) the spectral type based upon the new system; (4) a catalog symbol denoting binary membership; (5) a list of most names known to exist for a given star; (6) proper motion and position angle; (7) broad-band UBV Photometry, V, B-V, U-B; (8) multichannel spectrophotometry, V(MC), g-r; (9) Stroemgren narrow-band photometry y, b-y, u-b; (10) an absolute visual magnitude based upon the best available color-magnitude calibration or trigonometric parallax; (11) the observed radial velocity uncorrected for gravitational redshift or solar motion; and (12) the trigonometric parallax with mean error when available. A Notes section for unusual or peculiar stars and a coded Reference Key alphabetized by the first author's last name are presented, as well as an expanded table cross-referencing all names to catalog WD number. An introduction and full descriptions of the entries are provided in the text.
Data for stars WD White Dwarf (WD) number number=1 Stars having identical catalog numbers, whether binary or not, are distinguished by using the designations .1 and .2 in bytes 9-10 --- RAh Hours RA, Equinox=B1950, Epoch=1950.0 h RAm Minutes RA, Equinox=B1950, Epoch=1950.0 min RAs Seconds RA s PosFlag Coordinate accuracy flag number=2 PosFlag specifies the accuracy (and in some cases precision) to which the equatorial coordinates are given: 1: RA given in hours, minutes and seconds; Dec given in degrees, arcminutes, and tenths 2: RA originally in hours, minutes and tenths, which were converted to minutes and seconds; Dec given in degrees and whole minutes 3: RA originally in hours, minutes and tenths, which were converted to minutes and seconds; Dec given in degrees, minutes and tenths 4. RA given in hours, minutes and seconds; Dec given in degrees and whole arcminutes 5. RA originally in hours and whole minutes, seconds were entered as 00; Dec given in degrees and whole arcminutes --- DE- Declination sign --- DEd Degrees Dec, Equinox=B1950, Epoch=1950.0 deg DEm Minutes Dec, Equinox=B1950, Epoch=1950.0 arcmin SpType Spectral type (definitions in the paper, or in file "preface.tex"). --- bNote 'b' if white dwarf is member of binary, '*' indicates a note in file "notes.dat" --- --- Left bracket enclosing the reference --- r_SpType Reference code for spectral type --- --- Right bracket enclosing the reference --- Names Other names for this star, see table Names --- Vmag V or other magnitude (see n_Vmag) mag u_Vmag Uncertainty flag (:) on Vmag --- n_Vmag 'pg' if Vmag is a photographic magnitude, ' B' if Vmag is a B magnitude --- B-V B-V color in the UBV system mag u_B-V Uncertainty flag (:) on B-V color --- ColClass Color class from Lowell or Luyten PM surveys --- U-B U-B color in the UBV system mag u_U-B Uncertainty flag (:) on U-B color --- --- Left bracket enclosing the reference --- r_Vmag Wide band photometry reference code --- --- Right bracket enclosing the reference --- Vsphot V mag from multichannel spectrophotometry mag g-r g-r color from spectrophotometry mag u_g-r Uncertainty flag (:) on g-r --- --- Left bracket enclosing the reference --- r_Vsphot Multichannel spectrophotometry reference code --- --- Right bracket enclosing the reference --- ymag y mag from ubvy photoelectric observations mag b-y b-y color from uvby mag u-b u-b color from uvby mag --- Left bracket enclosing the reference --- r_ymag uvby photoelectric photometry reference code --- --- Right bracket enclosing the reference --- AbsMag Absolute visual magnitude mag x_AbsMag 'E' if AbsMag can be computed from Effective Temperature Teff, or uncertainty flag (:) on AbsMag number=3 For DO and DOZ white dwarfs, AbsMag is a directly derivable effective temperature value. These are given in units of 10^3^ K A ':' for uncertain AbsMag may appear also (WD 0736+053) --- --- Left bracket enclosing the reference --- n_AbsMag Method of calculation of AbsMag number=5 The codes to indicate the method of calculation of the absolute magnitude are: 1 = trigonometric parallax (>0.1arcsec) 2 = multichannel spectrophotometric colors 3 = uvby (Stroemgren) colors 4 = UBV photometry 5 = Teff value from Wesemael, Green and Liebert (1993PASP..105..761W), Werner and Heber (1992, in "The Atmospheres of Early-Type stars", ed. U. Heber & S. Jeffrey, Springer, p. 273) or Napiwotzki and Schonberner (1991, in "White Dwarfs", ed. G. Vauclair and E.M. Sion, NATO ASI Series, Series C, 336: Dordrecht, Kluwer, p. 39) 6 = Liebert, Dahn and Monet (1988ApJ...332..891L) 7 = Bergeron, Ruiz and Leggett (1997ApJS..108..339B) 8 = Liebert et al., (1997, in "White Dwarfs", ed. J.Isern, M. Hernanz & Garcia-Berro, Dordrecht: Kluwer, p. 85) 9 = Smith (1998, Ph.D Thesis, Florida Institute of Technology, Melbourne, FL.) --- --- Right bracket enclosing the reference --- pm Total proper motion arcsec/yr u_pm Uncertainty flag (:) on pm, or Estimated proper motion number=4 In cases where only an estimated proper motion is reported in the Lowell proper-motion surveys, the "pm" field is blank and a corresponding code is given there in "Epm" field. These codes are defined in Giclas et al. (1967, 1970) and are the following: 0: Stars of blue color whose motions are too small to definitely verify on all plates. 1: pm <= 0.1 arcsec/yr 2: 0.1 <= pm < 0.2 arcsec/yr 3: 0.2 <= pm < 0.26 arcsec/yr --- pmPA Position angle of proper motion vector deg --- Left bracket enclosing the reference --- r_pm Proper motion reference code --- --- Right bracket enclosing the reference --- RadVel Radial velocity km/s --- Left bracket enclosing the reference --- r_RadVel Radial velocity reference --- --- Right bracket enclosing the reference --- Plx Trigonometric parallax arcsec e_Plx Reported mean error of parallax mas --- Left bracket enclosing the reference --- r_Plx Parallax reference code --- --- Right bracket enclosing the reference --- Teff Effective temperature when x_AbsMag is 'E' kK Cross-identifications of White Dwarfs Name Common name of the object --- --- Prefix of catalog --- WD White Dwarf (WD) number --- Notes for stars flagged in "catalog.dat" --- Prefix of catalog, blank for continuation --- WD White Dwarf (WD) number --- Notes Text of note for this star --- References mentioned in file "catalog.dat" RefCode Reference code --- BibCode CDS/ADS/NED BibCode --- Text Text of reference --- preface.tex Introduction by G.P. McCook and E.M. Sion Nils Odegard SSDOO/ADC 1999 Jun 09 This 1998 version 2 of the White Dwarf Catalog by G. McCook and E.M. Sion last revision June 8, 1999 was copied from ftp://astro1.ast.vill.edu/pub/mccook/. III_210.xml Catalogue of Correspondences CSI/ADS/IDS 4006 IV/6 Catalogue of Correspondences CSI/ADS/IDS Catalogue of Correspondences CSI/ADS/IDS J Jung M Bischoff F Ochsenbein Bull. Inf. CDS No. 4, p. 27 ??? ??? 1973 1973BICDS...4...27J Cross identifications Stars, double and multiple This catalog of correspondences is a cross index for the the Catalog of Stellar Identifications (CSI) (Ochsenbein et al., 1981), the Aitken Double Star Catalog (ADS) (Aitken, 1932), and the Index Catalogue of Visual Double Stars (IDS) (Jeffers et al., 1963). Catalog records contain the main Durchmusterung identification (which is the key for the CSI), followed by the ADS identification and system component letter(s), and the star's coordinates (1900) from the IDS. The ADS identifier field is blank for non-ADS stars. The RA and Dec are not always listed when the star belongs to ADS.
Catalog Data DMsign Main Durchmusterung sign A negative zone (z) is replaced in the file by (-z + 90). --- DMzone Main Durchmusterung Zone --- DM DM Number Negative for non-DM stars. Stars without DM identification are listed at the end of each zone and have been given a fictitious DM identification, the number being the Right Ascension (Ep 1950.0) in tenths of minutes, times -1, and the zone in degrees, the code being 0. Single-digit zones are preceded by zeros such that byte 1 always contains a + or -. --- DM_cat Code for Durchmusterung Catalog O to 19 = BD (Bonner DM) 20 to 39 = CD (Cordoba DM) 40 to 59 = CPD (Cape Phot. DM) --- ID ADS Identification Field is left blank for non-ADS stars. --- ABC Component of the system A = component A of the system, etc. AB = components A and B, where separation < 3 arcmin, etc. Magnitude and coordinates are those of the brightest star of the grouping. --- RAh Right ascension (1950.0) hours taken from IDS RA and Dec are not always listed when the star belongs to ADS. h RAm Right ascension (1950.0) minutes min --- Right ascension (1950.0) tenth of min. dmin DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin James E. Gass & Julie Anne Watko SSDOO/ADC 1997 Mar 13 Special thanks are given to Francois Ochsenbein of CDS for his help in identifying format problems in the data file. UNKNOWN UNKNOWN March 1997 - Added Brief Description (James Gass, ADC) August 1996 - Corrected RA of 12451 AB from 27 42.5 to 19 22.5 (James Gass, ADC) August 1996 - Corrected RA of +10 1032 from 0 65.4 to 6 5.4 (James Gass, ADC) August 1996 - Separated RA minutes and tenths of minutes into two fields for the byte-by-byte table in this document (James Gass, ADC) IV_6.xml Cross Identifications of HDE Stars 4008 IV/8 Cross Identifications of HDE Stars Cross Identifications of HDE Stars R Bonnet CDS Bull. No. 14, p. 114 ??? ??? 1978 1978BICDS..14..114B III/155 : Second Henry Draper Exten.: Types, Positions 10639 Stars (Cannon+ 1949) III/135A : Henry Draper Catalogue and Extension (Cannon+ 1918-1924; ADC 1989) III/182 : HDE Charts: positions, proper motions (Nesterov+ 1995) Cross identifications Durchmusterungen This catalog provides cross identifications of the stars in the HDE (A.J. Cannon Memorial stars) to stars in the AGK2, Cape Photographic (CP), Cape Faint Stars (CD), or Bonner Durchmusterung (BD) catalogs. It is divided into two parts. The first part (part1.dat) cross-identifies stars in the AGK2, CP, and CD catalogs according to their HDE number and HDE spectral classes. The second part (part2.dat) cross-identifies additional BD stars to entries in the HDE charts. These are stars lacking an HDE spectral type. These tables include cross-identifications to the CSI catalog. These are stars that do not appear in any Durchmusterung, but are in the CSI. For such non-Durchmusterung (non-DM) stars, the author has built a "DM" number from the appropriate zone of the BD/CD/CP or from its 1950 declination, a negative number for its number in the zone, and a code that enables the separation of binaries.
Catalog Data, Part 1 HDE HDE identification (Harvard Annals 112) --- R Indicates entry in part2 --- DM DM identification Extra digits in columns 23 and 24 are for binaries. --- B B magnitude A colon (:) following magnitude values indicates uncertainties. mag Dble Where magnitudes are for multiple stars The original CDS document for this catalog states that "D" indicates that the magnitude(s) refer to a system of stars (binary or multiple). However there are no "D" entries in this field - only "V" entries. It is likely that V conveys a similar meaning, but this has not been confirmed. --- V V magnitude mag Sp HDE spectral class --- coords Coordinates (B1950) This field contains 1950 coordinates for some of the stars in the catalog. Some include decimal minutes, while most are entered as minutes and seconds. --- Catalog Data, Part 2 HDE HDE identifier (Harvard Annals 112) --- DM DM identification --- Name Variable name --- Double Double name with component designation --- James E. Gass SSDOO/ADC 1997 Mar 23 UNKNOWN UNKNOWN 03-Mar-1997: The exclamation points (!) that served as column separators in the original catalog data files were replaced with ASCII blanks by the ADC. 03-Mar-1997: Data files renamed from catalog.dat1 and catalog.dat2 to part1.dat and part2.dat. 03-Mar-1997: Standard document added by James Gass of ADC. IV_8.xml SAO-HD-GC-DM Cross Index 4012 IV/12 SAO-HD-GC-DM Cross Index SAO-HD-GC-DM Cross Index N G Roman W H Warren Jr. N J Schofield Jr. Astronomical Data Center ??? ??? 1983 1983 I/108 : Cape Photographic Durchmusterung (CPD) (Gill+ 1895-1900) I/113 : General Catalogue of 33342 stars (GC) (Boss 1937) I/114 : Cordoba Durchmusterung (CD) (Thome 1892-1932) I/119 : Southern Durchmusterung (BD) (Schoenfeld+ 1886) I/122 : Bonner Durchmusterung (BD) (Argelander 1859-62) I/131 : SAO Star Catalog J2000 (SAO Staff 1966; USNO, ADC 1990) III/135 : Henry Draper Catalogue and Extension (HD) (Cannon+ 1918-1924) III/182 : HDE Charts: positions, proper motions (Nesterov+ 1995) Morin, D. 1973, Table of Correspondences SAO/HD/DM/GC, Obs. de Meudon, unpublished Cross identifications The catalog is an updated, corrected, and extended version of a table of correspondences originally prepared by Morin (1973). The individual data corrections, additions, and changes included in the new version number 11398, with 8600 data records having at least one change. In addition to the correction of all errors found since preparation of the original catalog, most of which resulted from misidentifications and omissions of components in multiple-star systems and missing Durchmusterung numbers (the common identifier) in the SAO Catalog, component identifications from the Index Catalogue of Visual Double Stars (IDS) have been appended to all multiple SAO stars having the same DM numbers, and lowercase identifications for supplemental (footnoted) BD stars have been added. Stars deleted (duplicate entries) in the SAO Catalog have been appended with a "D" and their data removed, although the records have been kept (with SAO number only) in order not to change the number of SAO stars. The data include SAO number, HD number, HD multiplicity code, GC number, DM identification code (BD, CD, CP), and number. There are fewer objects than records because of the deleted entries appended with a "D" as described above (35 stars deleted). A microfiche listing all changes made by the ADC in the early 1980's is available on request. Please contact request@nssdca.gsfc.nasa.gov.
The SAO-HD-GC-DM Cross Index SAO SAO Catalog number --- RAh Hours RA, equinox J2000 h RAm Minutes RA, equinox J2000 min RAs Seconds RA, equinox J2000 s DE- Sign Dec, equinox J2000 --- DEd Degrees Dec, equinox J2000 deg DEm Minutes Dec, equinox J2000 arcmin DM Durchmusterung catalog ID the Durchmusterung identification is made of DMcode in bytes 20-21 ("BD", "CD" or "CP") DMzone in bytes 30-32 (zone in degrees) DMnumb in bytes 33-36 (running number in zone) DMsupp in byte 32 ("a" or "b" for additional stars) --- HD Henry Draper Catalog (HD) number --- m_HD HD number code (see comment) the multiplicity code contains: '0' Single star, or companion > 0.3 mag (visual) fainter than the primary to which the entry refers. '1' Brighter component with a companion <= 0.3 mag fainter. '2' Fainter component with a companion <= 0.3 mag brighter. '9' The SAO Catalog entry refers to two consecutive HD numbers, the lower of which is given. --- GC Boss General Catalog (GC) number --- adc.doc Documentation NSSDC/WDC-A-R&S 91-20 (ascii) adc.tex Documentation NSSDC/WDC-A-R&S 91-20 (LaTeX) Gail L. Schneider SSDOO/ADC Francois Ochsenbein CDS 1996 May 13 UNKNOWN UNKNOWN See the documentation, either in LaTex (doc.tex), or in plain ascii (adc.doc), section 3. The catalogue distributed on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992, Astronomical Data Center, NASA Greenbelt), directory /crossid/saohddm, contained two more data files not included here: the index sorted by right ascension and declination, and by HD numbers. IV_12.xml Liste des binaires spectroscopiques du fichier general de Toulouse (List of spectroscopic binaries from the Toulouse general catalogue) 4016 IV/16 List of Spectroscopic Binaries Liste des binaires spectroscopiques du fichier general de Toulouse (List of spectroscopic binaries from the Toulouse general catalogue) A Pedoussaut A Capdeville N Ginestet J -M Carquillat Observatoire de Toulouse ??? ??? 1985 1985 V/40 : 7th Orbital Elements of Spectroscopic Binaries (Batten+ 1978) V/64 : Eighth Orbital Elements of Spectroscopic Binaries (Batten+ 1989) V/49 : 14eme catalogue complementaire de binaires spectroscopiques V/60 : 15eme catalogue complementaire de binaires spectroscopiques Batten A.H., 1967, "Sixth catalogue of the orbital elements of spectroscopic binary systems" Publ. Dominion Astrophys. Obs., vol.XIII, n 8. Batten A.H., Fletcher J.M., Mann P.J., 1978, "Seventh catalogue of orbital elements of spectroscopic binary systems" Publ. Dominion Astrophys. Obs., vol.XV, n 5. Binaries, spectroscopic Cross identifications This catalogue lists the designations of the spectroscopic binaries in the Lick lists, in Batten's 6th and 7th catalogues, in the "Toulouse Catalogues Complementaires" 1-14, as well as the designation from general-purpose catalogues.
The list of Spectroscopic Binaries HD/DM HD or Durchmustering designation of the binary --- Name Other designation --- Lick Existence in Lick catalogues number=1 Values of: 181 = W.W. Campbell, 1910, University of California Publications LICK Observ.Bull. vol.VI, 181 355 = J.H. Moore, 1924, University of California Publications LICK Observ.Bulletin, vol.XI, 355. 521 = J.H. Moore, F.J. Neubauer, 1948, University of California Publications, LICK Observ.Dull. vol.XX, 521. --- Bat6 Designation in Batten's 6th Catalogue number=2 Identification in catalogue by A.H. Batten, 1967, The binaries preceded by RB are from the Table 2 "List of stars rejected from the catalogue" --- Bat7 Designation in Batten's 7th Catalog <V/40> --- Toulouse Number of the "Catalogues Complementaires" where the binary is quoted number=3 The "Catalogues Complementaires" are: 1: R.Bouigue, 1952, Ann. Obs. Toulouse XXI, 31 2: R.Bouigue, 1954, Ann. Obs. Toulouse XXII, 49 3: R.Bouigue, 1955, Ann. Obs. Toulouse XXIII, 45 4: R.Bouigue, 1956, Ann. Obs. Toulouse XXIV 5: R.Bouigue, 1957, Ann. Obs. Toulouse XXVA, 69 6: R.Bouigue, J.L.Chapuis, 1959, Ann. Obs. Toulouse XXVII 7: A.Pedoussaut, 1963, Ann. Obs. Toulouse XXIX, 31 8: A.Pedoussaut, 1964, Ann. Obs. Toulouse XXX, 49 9: A.Pedoussaut, 1965, Ann. Obs. Toulouse XXXI, 39 10: A.Pedoussaut, 1968, Ann. Obs. Toulouse XXXII 11: A.Pedoussaut, N.Ginestet, =1971A&AS....4..253P 12: A.Pedoussaut, J.M.Carquillat, =1973A&AS...10..105P 13: A.Pedoussaut, R.Nadal, =1977A&AS...27...55P 14: A.Pedoussaut, N.Ginestet, J.M.Carquillat, =1984A&AS...58..601P --- Francois Ochsenbein CDS 1996 Jul 29 The help of J.L. Halbwachs (CDS) and J. Jobard (Toulouse) for the construction and transformation into machine-readable form is acknowledged. IV_16.xml WDS-DM-HD-ADS Cross Index 4018 IV/18 WDS-DM-HD-ADS Cross Index WDS-DM-HD-ADS Cross Index N G Roman Astronomical Data Center ??? ??? 1987 1987 Stars, double and multiple Cross identifications A cross index of 1900 positions and discoverer names, DM numbers, HD numbers, and ADS numbers has been prepared for stars in the 1984 tape version of the Washington Catalog of Visual Double Stars (WDS). Five files are furnished so that any of these designations can be used to search the cross index. A file of discoverer names and numbers is included in the catalog for systems with multiple designations. All DM numbers given in the notes to the WDS have been transferred to the cross index, and many additional or corrected DM numbers have been inserted. Year 2000 positions are also given in the sort by 1900 positions.
A machine-readable version of the Washington Catalog of Visual Double Stars (WDS) was prepared in 1984 (Worley 1984) on the basis of a data file that has been collected and maintained for more than a century by a succession of double-star observers. Although this catalog is now being continually updated, a new copy for distribution is not expected to be available for a few years. The WDS contains DM numbers (Argelander 1859-1862, Gill and Kapteyn 1895-1900, Thome 1892-1932), but many of these are listed only in the notes, which makes it difficult to search for double-star information, except by position. Hence, a cross index that provides complete DM identifications is desirable, and it appears useful to add HD numbers (Cannon and Pickering 1918-1924, Cannon 1925- 1936) for systems in that catalog. Aitken Double Star (ADS) numbers (Aitken 1932) have been retained from the WDS, but no attempt has been made to correct these except for obvious errors. A major effort in the preparation of this cross index has been devoted to improving the DM designations. A subset of the information in the WDS has been prepared that lists the 1900 position, the double-star observer and number, the component designation, the DM number, and the ADS number. All DM numbers given only in the notes have been entered by duplicating the entry and changing the component designation appropriately. The standard rule for multiple systems in the catalog is that the DM number refers to the first component. This rule is frequently violated, however, so that it often appears that a single component has two different DM numbers. All such cases have been checked and the component designations have been corrected appropriately. It should be noted that the introduction to the 1984 machine-readable version of the WDS is in error: unless modified by the notes, DM numbers for the -52d zone refer to the CPD. In multiple systems with more than one discoverer name, numbers are sometimes given for components with one name and not for components with another, even though the magnitudes and spectral types indicate that the entries refer to the same star. In those cases in which the stars are well above the magnitude limit of the Durchmusterung (usually brighter than ninth magnitude), the DM catalog was searched for other stars that might be confused with the star identified in the WDS. If no such star was found, the DM number was entered for the second name as well. As part of the preparation for the HIPPARCOS project, a significant number of DM numbers has been found for WDS stars by position matches (Nys 1983; Bacchus 1983; Nys 1983; Bacchus and Nys 1985; Nys 1984). Many fainter components were located in the Cape Photographic Dtuchmusterung (CP) for systems north of -52d declination for which the brighter component is in the Cordoba Dllrchmusterung (CD). These DM assignments were also checked as far as possible, and most are included in the cross index. In the course of various checks, other errors were uncovered. Many, but by no means all of these, involved either supplemental stars in the northern hemisphere (Warren and Kress 1980) or catalog confusion in the southern hemisphere. To alleviate the latter problem in the future, catalog designations have been added for all DM numbers. Appendix B (on microfiche) lists all DM numbers that have been newly entered or changed from those in the WDS. Numbers given correctly in the notes to the WDS are not included. Using the improved DM listing, a correlation between a DM sort of the WDS and a DM sort of the HD was used to insert HD numbers for the appropriate systems. Stars for which WDS and HD listings differed in position by more than 3 minutes of arc in declination or 0.3 minutes of time in right ascension were investigated individually, often leading to the discovery of errors, which were corrected. The stars without DM numbers were then correlated with the HD by position, and the HD numbers were inserted if the magnitudes and spectral types agreed satisfactorily. For most of the position matches, the stars are sufficiently close to the magnitude limit of the HD, or the HD positions in crowded fields are sufficiently rough, that it is impossible to verify that the same star is referenced. For the few cases in which the identity appears highly likely, the HD number and, occasionally, the DM number from the HD have been added to the cross index. All position matches with the HD for WDS stars without DM numbers are listed in nodm.dat. For the WDS entries, table 8 gives the 1900 position, the discoverer name and number, and the magnitudes as given in the WDS; the HD data provided are the HD and DM numbers, the position, the visual magnitude, and the spectral type. If the HD does not give a visual magnitude, the photographic magnitude is given in italics. It proved impossible to resolve a few of the problems uncovered. These are listed in Table 1. In other cases, the resolution may not have been obvious, but a reasonably likely resolution was adopted. Care should be taken with multiple systems with two or more observer identifications. The WDS is not completely consistent either in assigning DM numbers to relatively bright stars or in assigning DM numbers to components in more than one subsystem. The proper DM number for the component, the DM number for the brightest component, or no DM number may be listed. An attempt has been made to clarify the assignment of the DM numbers when it appears likely that the same star is involved and no DM number is listed. Only in extreme cases have DM numbers been removed for components that are too faint to be in the DM catalogs. Although an attempt was made to assign the proper DM number to each component, there were some circumstances in which this was not done. If the magnitude of a component is ninth or fainter, if no magnitude is given in the WDS, or if there are several stars in the vicinity with approximately the same magnitude, the proper assignment is uncertain. In many systems a DM number is given for a secondary component, but it is apparent from the magnitudes that the number refers to the brightest component of the subsystem. If the primary of the subsystem is not included in the WDS for the same subsystem name, both the component designation and the DM number are retained as given in the WDS unless it is reasonably certain that the star is the same as that in another subsystem with a different DM number. Near the limit of the DM catalogs, especially, many components listed without DM numbers are probably actually DM stars. As for the DM numbers, HD numbers have been assigned to components listed in more than one subsystem when it appears likely that the same star is involved. However, particularly with HD numbers, it is often difficult to determine whether two stars with the same DM number really are the same star. names.dat lists all systems with multiple discoverer names and numbers, with all designations occurring in the system. It is sorted alphabetically and, within a discoverer designation, numerically. The systems are listed multiply so that the list may be entered with any designation. An attempt has also been made to assign HD numbers to the proper components when two HD numbers refer to the same DM number, but this is often impossible. In many cases, the assignment of two numbers in the HD is merely an indication that the spectrum is composite, and the assignment of the numbers to individual components is meaningless. Nevertheless, an assignment for at least one discoverer designation in a system is made to alert the catalog user to the existence of two numbers in the HD. In assigning HD numbers to components, the following criteria were used in descending order of priority: (1) the relative position, in the few cases in which the HD lists different positions; (2) spectral type; (3) magnitude; and (4) position angle (that is, the earlier HD number is presumed to be the western component, although in many cases it is clear that the HD could not distinguish which component is the western one). Table 2 lists multiple HD numbers for systems with the same DM number which are not given in the Cross Index. All changes in the cross index other than those in the DM number are listed in Table 3. The references for the changes listed in the column headed "S" of Appendix B and Table 3 are as follows: 1. Abt, H. A. 1978, private communication. 2. Nys, O. 1983, Bull. Inform. CDS No. 24, p. 53. 3. Bacchus, P. 1983, Bull. Inform. CDS No. 25, p. 23. 4. Nys, O. 1983, Bull. Inform. CDS No. 25, p. 27. 5. Bacchus, P. and Nys, O. 1985, Bull. Inform. CDS No. 29, p. 43. 6. Nys, O. 1984, Bull. Inform. CDS No. 26, p. 53. 7. ADC. 8. ADC, confirmed in updated WDS file (Worley, private communication). Note that many other Changes attributed to the ADC are also included in the updated WDS, but these have not been checked. For the most part, if a component had a letter designation in the WDS, this is retained to alert the cross index user to the fact that the system may have more than two components. If a DM number is listed in the notes for B in a two-component system, A has been added for the primary component to distinguish between A and B. The revision of the WDS currently in progress replaces the 1900 positions by J2000 positions. To facilitate the use of this cross index at a later date, equinox 2000 positions are also included in 2000.dat. They may not agree exactly with the new catalog positions, since proper motions are not applied; but, except for systems with very high proper motions, they should allow the user to locate the systems in the newer catalog. Five stars in the WDS have no discoverer designations. Worley has since provided "names" for these systems. These are listed in Table 4 and are included in the cross index.
The index, sorted by 1900 position with 2000 positions RAh Right Ascension hours (1900) h RAdm Right Ascension deci-minutes dmin DE- Sign of declination --- DEd Declination degrees (1900) deg DEm Declination minutes (1900) arcmin RAh2000 Right Ascension hours (2000) h RAdm2000 Right Ascension deci-minutes dmin DE-2000 Sign of declination --- DEd2000 Declination degrees (2000) deg DEm2000 Declination minutes (2000) arcmin disc Discoverer designation --- num Discoverer number --- comp Component --- DMcat Durchmusterung (DM) catalog designation BD=Bonner Durchmusterung; CD=Cordoba Durchmusterung; CP=Cape Photographic Durchmusterung). All DM fields are blank if DM number is missing --- DM- Sign of DM zone --- DMz DM zone deg DMno DM number --- suppl Supplement designation --- HD HD number --- ADS ADS number --- Index sorted by discoverer name and no. disc Discoverer designation --- num Discoverer number --- comp Component --- RAh Right Ascension hours (1900) h RAdm Right Ascension minutes (1900) dmin DE- Sign of declination --- DEd Declination degrees (1900) deg DEm Declination minutes (1900) arcmin DM Durchmusterung (DM) catalog designation See Note on DMcat, file position.dat --- DM- Sign of DM zone --- DMz DM zone deg DMno DM number --- suppl Supplement designation --- HD HD number --- ADS ADS number --- Index sorted by DM number DM Durchmusterung (DM) catalog designation See Note on DMcat, file position.dat --- DM- Sign of DM zone --- DMz DM zone deg DMno DM number --- suppl Supplement designation --- disc Discoverer designation --- num Discoverer number --- comp Component --- RAh Right Ascension hours (1900) h RAdm Right Ascension deci-minutes dmin DE- Sign of declination --- DEd Declination degrees (1900) deg DEm Declination minutes (1900) arcmin HD HD number --- ADS ADS number --- Index sorted by HD number HD HD number --- disc Discoverer designation --- num Discoverer number --- comp Component --- RAh Right Ascension hours (1900) h RAdm Right Ascension deci-minutes dmin DE- Sign of declination --- DEd Declination degrees (1900) deg DEm Declination minutes (1900) arcmin DM Durchmusterung (DM) catalog designation See Note on DMcat, file position.dat --- DM- Sign of DM zone --- DMz DM zone deg DMno DM number --- suppl Supplement designation --- ADS ADS number --- Index sorted by ADS number ADS ADS number --- disc Discoverer designation --- num Discoverer number --- comp Component --- RAh Right Ascension hours (1900) h RAdm Right Ascension deci-minutes dmin DE- Sign of declination --- DEd Declination degrees (1900) deg DEm Declination minutes (1900) arcmin DM Durchmusterung (DM) catalog designation See Note on DMcat, file position.dat --- DM- Sign of DM zone --- DMz DM zone deg DMno DM number --- suppl Supplement designation --- HD HD number --- Systems with multiple names RAh Right Ascension hours (1900) h RAdm Right Ascension deci-minutes dmin des1 First designation --- des2 Second designation --- des3 Third designation --- des4 Fourth designation --- des5 Fifth designation --- des6 Sixth designation --- des7 Seventh designation --- Nancy Grace Roman ADC/SSDOO 1996 Dec 27 IV_18.xml Cordoba/Cape Durchmusterungen Cross Index 4019 IV/19 Cordoba/Cape Durchmusterungen Cross Index Cordoba/Cape Durchmusterungen Cross Index B N Rappaport W H Warren Jr. unpublished ??? ??? 1987 1987 Cross identifications Durchmusterungen The fact that there are two durchmusterungen covering the southern sky means that there is frequently a problem identifying a star with a number in one catalog with that in another. To make this process easier, a cross index has been prepared giving corresponding numbers for the same star. This catalog contains two files, one sorted by Cordoba number and the other sorted by Cape Photographic number.
NOTE: Because the two durchmusterungen have been made in different colors, near the limiting magnitude, stars in one catalog may not appear in the other. This, coupled with comparatively crude positions means that for some stars, there will be one star in one catalog and two stars, equally probable to be the corresponding star, in the other catalog. The undersigned spent some time trying to resolve these problems and concluded that, for more than 100 stars, the assignment was impossible. Dr. Warren has informed me that he believes that he has resolved a few additional problems and wants to work further on the cross index. He also states that there are a number of cases in which the positions in the two catalogs are sufficiently different that they may not refer to the same star. However, he seems to have made little progress for several years. Since the cross index will be generally useful, the undersigned decided that it was more important to distribute it as it is than to hold it longer. The user should be aware of possible problems.
The cross index in CPD order cpz Zone in the Cape Photographic Durchmusterung --- cpn Number in the CPD --- cps Supplemental letter code in CPD Supplemental letter codes are lower case characters (e.g.,"a") as used in the Bonner Durchmusterung for inserted stars. --- cpbl The number 9 indicates a blend of two stars in CPD --- cdz Zone in the Cordoba Durchmusterung --- cdn Number in the CD --- cds Supplemental letter code in CD --- cdbl The number 9 indicates a blend of two stars in CD --- uncer Colon indicates uncertain identification Uncertainty (colon) codes usually mean that two stars in one DM are equidistant from one star in the other catalog. The available information indicates that the stars indicated are the most likely identification, but this is uncertain. Preferences are generally based on systematic positional differences for nearby stars. Magnitudes cannot usually be used unless color information is available. --- dif The difference in position in the two durchmusterungen arcmin The cross index in CD order cpz Zone in the Cordoba Durchmusterung (CD) --- cpn Number in the CD --- cps Supplemental letter code in CD Supplemental letter codes are lower case characters (e.g.,"a") as used in the Bonner Durchmusterung for inserted stars. --- cpbl The number 9 indicates a blend of two stars in CD --- cdz Zone in the Cape Photographic Durchmusterung --- cdn Number in the CPD --- cds Supplemental letter code in CPD --- cdbl The number 9 indicates a blend of two stars in CPD --- uncer Colon indicates uncertain identification Uncertainty (colon) codes usually mean that two stars in one DM are equidistant from one star in the other catalog. The available information indicates that the stars indicated are the most likely identification, but this is uncertain. Preferences are generally based on systematic positional differences for nearby stars. Magnitudes cannot usually be used unless color information is available. --- dif The difference in position in the two durchmusterungen arcmin Nancy G. Roman ADC/SSDOO 1996 Nov 12 The undersigned thanks Drs. Rappaport and Warren for providing the cross index data. UNKNOWN UNKNOWN The original cross index was prepared by Rappaport on the basis of a machine match of positions. This was carefully reviewed by Warren who investigated many questionable identifications. Roman then studied many particularly questionable cases. As noted above, it is probably impossible to resolve all of these. IV_19.xml Infrared Source Cross Index 4021 IV/21 Infrared Source Cross Index Infrared Source Cross Index M Schmitz J M Mead D Y Gezari NASA Ref. Publ. 1182 ??? ??? 1987 1987NASAR1182....0S Infrared sources The Infrared Source Cross-Index is a listing of correlated infrared source names (and positions) for astronomical objects observed at 1-1000 microns. The source names have been obtained from the data base of the first edition of the Catalog of Infrared Observations (NASA RP 1118), covering observations published through 1982. Additional identifications were located by correlating these names with identifications contained in other machine-readable astronomical catalogs in the NASA National Space Science Data Center. This cross index contains some 80,000 different source names for over 27,000 unique infrared sources. The catalog contains the 1950 position for each object as well as designations from the following catalogs: IRAS, Two-Micron Sky Survey, Air Force Geophysical Laboratory, The Henry Draper, a Durchmusterung, the Bright Star Catalog, the Boss General Catalog, the Dearborn Observatory, and the Smithsonian Astrophysical Observatory.
Catalog Data pre OBJECT NAME PREFIX from constellation --- name OBJECT NAME ROOT Object name as given in the Catalog of Infrared Observations. For object IDs derived from constellation names, the constellation name abbreviation is given in this field. --- RAh RIGHT ASCENSION hours (1950.0) h RAm RIGHT ASCENSION minutes min RAs RIGHT ASCENSION seconds Precision depends on original catalog precision. s DE- DECLINATION Sign (1950.0) --- DEd DECLINATION degrees deg DEm DECLINATION arcminutes arcmin DEs DECLINATION arcseconds arcsec n_ALIAS ALIAS FLAG If a decimal point ". n appears in this byte, then the object can also be found listed in the OBJECT NAME under the following name. --- ALIAS ALIAS Additional names for object --- IRAS IRAS IDENTIFICATION Cross-identifications with the IRAS catalogs are given in this field. Entries without a prefix are from the Point Source Catalog. Names with a leading "X" are from the IRAS Small Scale Structure Catalog. --- n_IRC CalTech TWO-MICRON SKY SURVEY FLAG If a decimal point "." appears in this byte, then the object can also be found listed in the OBJECT NAME under the following ID. This note applies to all flags that follow unless specified otherwise. --- IRC CalTech TWO-MICRON SKY SURVEY ID --- n_AFGL AIR FORCE GEOPHYSICS LAB FLAG --- AFGL AIR FORCE GEOPHYSICS LABORATORY ID An identification with the Air Force Geophysics Laboratory Survey (AFGL) is given in this field. An "S" appears in column 85 if the ID is from the AFGL Supplement series. --- n_HD HENRY DRAPER CATALOG FLAG --- EHD E = OBJECT IN THE HD EXTENSION --- HD HENRY DRAPER CATALOG ID An identification with the Henry Draper (HD) catalog is given in this field. An "E" appears in column 88 if the ID is from the HD Extension. --- n_DM DURCHMUSTERUNG CATALOG FLAG --- DM DURCHMUSTERUNG CATALOG ID An identification with one of the Durchmusterung catalogs is given in this field. The catalogs identified are: Bonner Durchmusterung (BD) Cordoba Durchmusterung (CCD) Cape Photographic Durchmusterung (CP) --- DMz DURCHMUSTERUNG ZONE deg DMno DURCHMUSTERUNG NUMBER --- n_BS YALE BRIGHT STAR CATALOG FLAG --- BS YALE BRIGHT STAR CATALOG ID --- n_GC BOSS GENERAL CATALOG FLAG --- GC BOSS GENERAL CATALOG ID --- n_DO DEARBORN OBSERVATORY FLAG --- DO DEARBORN OBSERVATORY CATALOG ID --- n_SAO SAO FLAG --- SAO SAO CATALOG ID --- Julie Anne Watko SSDOO/ADC 1995 Dec 12 IV_21.xml FK5 - SAO - HD - Common Name Cross Index 4022 IV/22 FK5 - SAO - HD - Common Name Cross Index FK5 - SAO - HD - Common Name Cross Index W B Smith unpublished ??? ??? 1996 1996 Astrometric data cross indentifications The author has combined data from various catalogs to produce a cross index of the numbers in the FK5, SAO, and HD catalogs. He has also added the Bayer or Flamsteed designations and the common or variable star names.
The catalog fk5 The FK5 number --- RAh Right Ascension hours (J2000) h RAm Right Ascension minutes (J2000) min RAs Right Ascension seconds (J2000) s pmRA- Sign of proper motion in RA --- pmRA Proper motion in right ascension 0.01s/yr DE- Declination sign --- DEd Declination degrees (J2000) deg DEm Declination minutes (J2000) arcmin DEs Declination seconds (J2000) arcsec pmDE- Sign of proper motion in declination --- pmDE Proper motion in declination 0.01arcsec/yr epRA Epoch for right ascension -1900 yr epDE Epoch for declination -1900 yr V Visual magnitude mag sp Spectral type --- DMcat DM catalog --- DMz DM zone --- DMno DM number --- SAO SAO number --- HD HD number --- BFno Bayer or Flamsteed number --- name Common name or variable name --- Nancy Grace Roman ADC/SSDOO 1996 Aug 31 The author thanks Patrick Wallace, Starlink Project Manager at the Rutherford Appleton Laboratory for both continuing guidance and counsel and for spot checking the catalog for accuracy. The author can be reached at Lone Star Observatory, 1133 Airline Drive, Grapevine, Texas, USA. His e-mail address is wbsjets@onramp.net. This catalog may not be published in whole or in part for commercial purposes without the written permission of the author. IV_22.xml Data for FK4/FK4 Supplement Stars 5003 V/3 FK4/FK4 Supplement Data Data for FK4/FK4 Supplement Stars D Morin CDS Bull. No. 4, p. 4 ??? ??? 1973 1973BICDS...4....4M Positional data Proper motions Parallaxes, trigonometric Radial velocities Spectral types This catalog provides additional data for FK4 and FK5 stars. Specifically, it contains the GC numbers and the HD numbers where available. It also contains the parallaxes from the Yale Catalogue of Trigonometric Parallaxes, various information from Wilson's General Catalogue of Stellar Radial Velocities, and positions and proper motions in galactic coordinates.
The data have been taken in the following catalogues: FK4 Fourth Fundamental Catalogue carried out under the supervision of W. Fricke and A. Kopff, Heidelberg (1963) FK4/SUP General Catalogue of 33,342 Stars for the Epoch 1950.0 Boss B., Carnegie Institution of Washington (1937) YP Yale Catalogue of Trigonometric Parallaxes Jenkins F., Yale University Observatory (1952, Suppl. 1963) WILSON General Catalogue of Stellar Radial Velocity Wilson R.F., Carnegie Institution of Washington, 601 (1953) BS Yale Catalogue of Bright Stars Hoffleit D., Yale University Obs. (1964) HD Henry Draper Catalogue Cannon A.J., Pickering B.C. (1924) comp. data have been computed
Data FK4 FK4 number --- GC GC number --- mag1 Visual magnitude (HD, FK4) blank for some variable stars mag Sp_HD HD spectral type (HD, FK4) --- RAh Right ascension (1950.0) hours (FK4) h RAm Right ascension (1950.0) minutes (FK4) min RAs Right ascension (1950.0) seconds (FK4) s DE- Declination (1950.0) sign (FK4) --- DEd Declination (1950.0) degrees (FK4) deg DEm Declination (1950.0) arcminutes (FK4) arcmin DEs Declination (1950.0) arcseconds (FK4) arcsec pmRA Proper motion in RA (FK4 + comp.) arcsec/a pmDE Proper motion in Dec (FK4 + comp.) arcsec/a e_pmRA Mean error on pmRA (FK4 + comp.) absent for FK4 sup stars 10-4arcsec/a e_pmDE Mean error on pmDE (FK4 + comp.) absent for FK4 sup stars 10-4arcsec/a Plx Parallax (YP) arcsec PEPlx Probable error on Plx (YP) 10-3arcsec mag2 Visual magnitude (WILSON) mag n_mag2 Remark about mag2 (WILSON) V = variable P = photographic --- Sp_W Spectral classification (WILSON) --- RV Radial Velocity (WILSON) km/s Q Quality from A to E (WILSON) --- Glon Galactic longitude (comp.) deg Glat Galactic latitude (comp.) deg pml Proper motion in galactic longitude computed from pmRA and pmDE arcsec/a pmb Proper motion in galactic latitude arcsec/a Sp_BS Spectral classification (BS) --- HD HD number --- Julie Anne Watko SSDOO/ADC 1996 Mar 29 V_3.xml Colours, Luminosities, and Motions of the Nearer Giants of Types K and M 5005A V/5A Colours, Luminosities, and Motions Nearer K-M Giants Colours, Luminosities, and Motions of the Nearer Giants of Types K and M O J Eggen Royal Obs. Bull. No. 125 ??? ??? 1966 1966QB4.G85n125.... Colors Space velocities Stars, giant Stars, late-type The data compilation Colours, Luminosities and Motions of the Nearer Giants of Types of K and M (Eggen 1966) contains all stars in the Yale Catalogue of Bright Stars (Hoffleit 1964) that have visual magnitudes brighter than 5.5 and that have been observed to have B-V redder than +0.8 mag, with the exception of a few K-type dwarfs. In addition to mostly K- and M-type giants, a few subgiants and supergiants are included. The data result from some 1600 photoelectric observations of 600 stars with the 50.8-cm reflector of the Hale Observatories. Approximately one-third of the stars had been observed at the Cape Observatory (Cousins and Stoy 1963). Although spectral types are given in the published catalog, they were taken from a variety of sources, are very inhomogeneous, and are not included in this catalog.
Catalog Data HR HR number from the Yale Catalogue of Bright Stars (Hoffleit 1964). --- HR2 A slash (/) and additional digit if a second HR star is included in the measurements. --- flag1 An asterisk (*) is present if there are remarks in the published catalog. --- GCRV GCRV number in the General Catalogue of Stellar Radial Velocities (Wilson 1953). --- GCRV2 A slash and additional digit if a GCRV star is included in the value given --- V Photoelectric V(E) magnitude. The precision varies within the data field. mag flag2 A "v" if the magnitude is variable; a colon (:) for uncertainty. If the magnitude given is considered to be a maximum, a code M is given in byte 46. --- B-V B-V color. The precision varies. mag flag3 uncertainty flag: colon (:) for uncertainty, "V" for variable. --- U-B U-B color. The precision varies. mag flag4 U-B flag (see byte 32). A question mark (?) is present if the value is surrounded by parentheses in the published table. --- ObsNum Number of observations, n, for UBV data. --- UBVcode Code for UBV measurements Code for UBV measurements C observed at the Cape Observatory (Cousins and Stoy 1963) H observed with the 100" telescope (no number of observations given) M variable magnitude reported is considered to be a maximum value for the variable star --- M(V) Absolute visual magnitude, M(V), taken from various sources, as indicated by the codes in bytes 53-54. Precision varies. mag flag5 Flag for M(V) Flag for M(V): : M(V) uncertain ? M(V) very uncertain No source is given for very uncertain values, nor for many of the other values quoted (53-54 blank). --- Source Source of M(V) Source of M(V), as denoted by the following codes: Cp available photometry of common proper-motion companion used to obtain distance moduli and luminosities H luminosity derived from probable membership in the Hyades group Tr not defined in source reference W Calibration of M(V) (W) used to derive M(V) (see page E152 of source reference) * values obtained by Gyldenkerne (1964) from photoelectrically determined luminosity parameters The source is not defined in the absence of a code. --- u- Sign of U component --- u U component of the space velocity relative to Sun. km/s u_u Colon if U uncertain. --- v- Sign of V component --- v V component of the space velocity km/s u_v Colon (:) if V uncertain. --- w- Sign of W component --- w W component of the space velocity km/s u_w Colon (:) if W uncertain. --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Aug 16 UNKNOWN UNKNOWN The original ADC documentation by Warren, Jr. (1986) was used to generate this ReadMe file. The data compilation Colours, Luminosities and Motions of the Nearer Giants of Types K and M was received on magnetic tape from the Centre de Donnees Astronomique, Strasbourg (CDS) on 9 July 1980. Text records at the beginning of the original file indicated that the data were punched in 1972 November at the Kanazawa Institute of Technology. The following modifications were made to the data file to standardize the format, to make the data easier to machine process (e.g., to separate character and numerical data fields) and to effect closer agreement between the published table and the machine format. 1. A catalog number "5005A74" assigned by the CDS was removed from the beginning of each record. Thirty-two text records containing a column (not byte) description and possible format for reading the data were removed entirely from the file, since their presence would have made the file more complicated to machine process and not sortable. 2. The remarks flag (byte 7) was moved from byte 5 so that it always occurs in the same position. This was previously not the case because of the data in bytes 5-6. 3. Decimal points were added to all V(E), B-V, U-B and M(V) data, the variability indicator "V" for V(E) was changed to lowercase "v", and plus signs were added to all positive values of B-V, U-B, M(V), U, V, and W. 4. The code "C" for number of observations was moved from byte 45 to byte 46 (to remove it from the numerical field) and the codes "H" and "M" for 100" and "max." occurring in the published table, were added. 5. The question mark for M(V) was moved from one of the sources bytes (53) to byte 52 to isolate it from the sources codes. The M(V) source codes CP and TR were changed to Cp and Tr, respectively, to agree with the published table. 6. The last five stars (HR 9066-9089) were missing from the file -- these were added. A few errors were found in the data during the course of this work and have been corrected, but the machine version has not been proofread. Therefore, if unusual values are found in the machine version, they should be checked against the published table before any interpretation is made. -------------------------------------------------------------------------------- V_5A.xml Space Velocity Catalogue 5008 V/8 Space Velocity Catalogue Space Velocity Catalogue O J Eggen Royal Obs. Bull. No. 51 ??? ??? 1962 1962RGOB...51...79E Space velocities New "post-1900" proper motions have been derived for all of the stars with known radial velocity of quality class A or B that are also contained in the General Catalog (GC, catalog <I/113>). The catalog lists the space motion vectors of the 3483 stars for which the differences between the pre- and post-1900 proper motions and the probable error of the combined values are small enough to cause less than about 5 km/s uncertainty in the total space motion based on the best available determinations of the stellar distances. In addition to the weighted means of the pre- and post-1900 proper motion components on the N30 system, the best available values of the radial velocity and the space-velocity vectors (UVW), based on these motions and on an assumed luminosity derived from considerations of all available estimates. Compared to the Table 1 of the publication, note that the following elements are missing: - the 3rd designation of Column I - the spectral classifications of Column III - all annotations of Column VIII: the uncertainty flag related to the distance modulus m-M, and also the annotations about binarity or clustering.
Table 1 HD HD Cat. <III/135> designation --- GC GC Cat. <I/113> designation --- Vmag Visual magnitude mag B-V color index mag U-B (or (U-B)c) color index mag pmRA Proper motion in right ascension number=1 Proper motions are converted to N30 system (Morgan H.R., 1952, Astron. Papers Amer. Ephemeris 13, see catalog <I/80>) 10-4s/a pmDE Proper motion in declination number=1 Proper motions are converted to N30 system (Morgan H.R., 1952, Astron. Papers Amer. Ephemeris 13, see catalog <I/80>) mas/a RVel Radial velocity from Wilson's GCRV Cat. number=2 Radial velocities from the "General Catalogue of Stellar Radial Velocity", Wilson R.F., 1953 (see catalog <III/21>) km/s q_RVel Quality index on RVel number=2 Radial velocities from the "General Catalogue of Stellar Radial Velocity", Wilson R.F., 1953 (see catalog <III/21>) --- pe(pm) Probable error on proper motions number=1 Proper motions are converted to N30 system (Morgan H.R., 1952, Astron. Papers Amer. Ephemeris 13, see catalog <I/80>) mas/a Uvel Component of space velocity number=3 The space velocity components are oriented: Uvel away from the Galactic centre Vvel in the direction of the galactic rotation Vvel in the direction of the North Galactic Pole km/s Vvel Component of space velocity number=3 The space velocity components are oriented: Uvel away from the Galactic centre Vvel in the direction of the galactic rotation Vvel in the direction of the North Galactic Pole km/s Wvel Component of space velocity number=3 The space velocity components are oriented: Uvel away from the Galactic centre Vvel in the direction of the galactic rotation Vvel in the direction of the North Galactic Pole km/s DUvel Change of Uvel with distance number=4 these numbers represent the changes in the values of (Uvel, Vvel, Wvel) caused by an increase of 1kpc in the assumed distance. km/s/kpc DVvel Change of Vvel with distance number=4 these numbers represent the changes in the values of (Uvel, Vvel, Wvel) caused by an increase of 1kpc in the assumed distance. km/s/kpc DWvel Change of Wvel with distance number=4 these numbers represent the changes in the values of (Uvel, Vvel, Wvel) caused by an increase of 1kpc in the assumed distance. km/s/kpc x Direction cosine of the radial velocity number=5 These direction cosines can be computed from the old galactic coordinates l (longitude) and b (latitude) by: x = -cos(b).cos(l) y = cos(b).sin(l) z = sin(b) 10-3 y Direction cosine of the radial velocity number=5 These direction cosines can be computed from the old galactic coordinates l (longitude) and b (latitude) by: x = -cos(b).cos(l) y = cos(b).sin(l) z = sin(b) 10-3 z Direction cosine of the radial velocity number=5 These direction cosines can be computed from the old galactic coordinates l (longitude) and b (latitude) by: x = -cos(b).cos(l) y = cos(b).sin(l) z = sin(b) 10-3 m-M Distance modulus number=6 the distance modulus (m-M) is related to the distance r expressed in kpc by: 5.log(r) = (m-M) - 10 mag Francois Ochsenbein CDS 1996 Jun 25 UNKNOWN UNKNOWN The catalogue was originally keypunched in November 1972 in K.I.T. computer center. The original version contained a first introduction (52 lines), and one star information laid over 3 cards. It has been transformed into a one-line per star at CDS in 1996; numerous misalignments in the data columns were also corrected in the course of this transformation. V_8.xml New Kinematic Data for Bright Southern OB Stars, Table 2: Kinematic Data, Table 4: Combined Proper Motions 5009A V/9A New Kinematic Data for Bright Southern OB Stars New Kinematic Data for Bright Southern OB Stars, Table 2: Kinematic Data, Table 4: Combined Proper Motions J R Lesh Astron. & Astrophys. Suppl. 5 129 1972 1972A&AS....5..129L Stars, OB Stars, bright Stars, distances Magnitudes, absolute Radial velocities Proper motions Distance moduli and distances (based on the MK spectral types of Hiltner et al., 1969, and UBV photometry from the Royal Observatory, Cape of Good Hope), new proper motions on the FK4 system, and newly evaluated and averaged radial velocities are presented for 440 bright O and B stars south of declination -20 deg. Proper motions combining the new and GC proper motions are also included.
Kinematic and Proper Motion Data HDpre "HD" label --- HD HD number --- V V magnitude mag u_V Uncertainty flag on V '*' if V is uncertain (variability or duplicity) --- B-V (B-V) colour index mag u_B-V Uncertainty flag on B-V --- m-M Distance modulus mag u_m-M Uncertainty flag on m-M --- r Distance of the star pc u_r Uncertainty flag on r --- RAh Right ascension (1950) hours h RAm Right ascension (1950) minutes min RAs Right ascension (1950) seconds s DE- Declination (1950) sign --- DEd Declination (1950) degrees deg DEm Declination (1950) arcminutes arcmin DEs Declination (1950) arcseconds arcsec pmRA New proper motion Right Ascension 10-5s/a e_pmRA Probable error on pmRA 10-5s/a pmDE New proper motion Declination 10-4arcsec/a e_pmDE Probable error on pmDE 10-4arcsec/a pmRA2 Corrected value: pmRA*cos(DE) 10-4arcsec/a pmDE2 Corrected value: pmDE 10-4arcsec/a RV Radial velocity (the "best estimate") km/s e_RV Probable error on RV km/s pmRA_com Combined proper motion in RA a weighted mean between the new and GC proper motions. 10-4arcsec/a pmDE_com Combined proper motion in Dec 10-4arcsec/a Julie Anne Watko SSDOO/ADC 1996 Apr 30 UNKNOWN UNKNOWN This catalogue combines the previous versions of ADC Cats V/9 and V/10. V_9A.xml Catalogue of High Velocity Stars 5011 V/11 Catalogue of High-Velocity Stars Catalogue of High Velocity Stars O J Eggen Royal Obs. Bull. No. 84, No. 111 ??? ??? 1964,1965 1964RGOB...84..111E Stars, high-velocity A catalogue is given of 656 stars which have space motions probably exceeding 100km/s with respect to the Sun. In addition to the apparent motions, many of which are new determinations, the catalogue contains the space velocity vectors UVW and other parameters, such as spectral type and color.
Catalog Data RAh Right Ascension 1950 (hours) h RAdm Right Ascension 1950 (deci-minutes) 0.1min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Id1 First identification number=1 The identification is coded on 13 characters: 1-3 = name of catalogue : blank for HD, W for Wilson's GCRV; other abbreviations aRE LTT, LDS, etc, 4-10 = number in the catalogue 11-13 = multiplicity (A, AB, etc...) --- Id2 Second identification number=1 The identification is coded on 13 characters: 1-3 = name of catalogue : blank for HD, W for Wilson's GCRV; other abbreviations aRE LTT, LDS, etc, 4-10 = number in the catalogue 11-13 = multiplicity (A, AB, etc...) --- Sp Spectral type number=2 The spectral type is coded on 12 characters: 1-2 = luminosity class (G, SG, D, SD, C ...) 3-4 = type and sub-type 5-10 = luminosity class 11-12 = peculiarities --- mV V magnitude 0.01mag n_V Remark on V (variability, duplicity...) --- B-V Colour index 0.01mag U-B Colour index 0.01mag n_U-B Remark on U-B: ":" for uncertainty on B-V ")" when U-B in Cape system (U-B)c --- RV Heliocentric Radial velocity, mainly from Wilson 0.1km/s q_RV Quality index on RV (A=good, D=poor) --- m-M Distance modulus 0.01mag u_m-M Uncertainty flag (:) on distance modulus --- N Running number --- pmra proper motion in RA number=3 The values of proper motions are those which are listed in line 5 of the original catalogue (reduced to N30 system). 0.1ms/a pmde proper motion in Dec number=3 The values of proper motions are those which are listed in line 5 of the original catalogue (reduced to N30 system). mas/a U U-component of the spatial velocity (toward galactic anticenter) km/s V V-component of the spatial velocity (toward galactic rotation) km/s W W-component of the spatial velocity (toward North galactic pole) km/s R1 Apogalactic distance of the galactic orbit 100pc R2 Perigalactic distance of the galactic orbit 100pc e Eccentricity of the galactic orbit, in 0.01 % Francois Ochsenbein CDS James Gass SSDOO/ADC 1997 Jul 31 UNKNOWN UNKNOWN The file was keypunched at CDS. A few errors (mainly misalignements) were corrected in June 1993 for the following running numbers: 69 105 123 144 276 284 285 310 V_11.xml Probable Members of the Small Magellanic Cloud 5013A V/13A Probable Members of the SMC Probable Members of the Small Magellanic Cloud M Azzopardi J Vigneau Astron. Astrophys. Suppl. Ser. 22 285 1975 1975A&AS...22..285A Probable Members of the Small Magellanic Cloud M Azzopardi J Breysacher Astron. Astrophys. 75 120 1979 1979A&A....75..120A V/78 : Catalogue of the Objects in the direction of the Small Magellanic Cloud (Bischoff et al., 1988) J/A+AS/97/603 : Carbon Stars in Small Magellanic Cloud (Rebeirot et al., 1993) J/A+AS/102/451 : H-alpha emission-line stars and PNs in Small Magellanic Cloud (Meyssonnier & Azzopardi, 1993) J/A+AS/113/539 : Suvery of Carbon Stars in Small Magellanic Cloud (Morgan & Hatzidimitriou, 1995) Magellanic Clouds An objective prism survey was conducted to discover probable members of the Small Magellanic Cloud. Interference filters were used to restrict the wavelength range and, hence, decrease the background and crowding. The limiting absolute magnitude of the survey is about -4.5. The 1975 paper listed 506 stars that show high luminosity characteristics; 193 of them had been confirmed by other authors. The 1979 paper added 14 additional probable members and photometric observations of 11 stars from the earlier paper that confirmed their membership. For completeness, four new Wolf-Rayet stars detected by Azzopardi and Breysacher (1979) were included. The catalog contains a catalog number in order of right ascension with the suffixes "a" or "b" used for the newer stars interpolated in the original list. Also included are the 1975 position, the MK spectral classification, the V magnitude, the (B-V) and (U-B) color indices, the number of observations, the identification chart number, and remarks indicating previous identifications. A later catalogue of the Small Magellanic Could star members is also published by Azzopardi and Vigneau =1982A&AS...50..291A Nomenclature Note: The stars from this paper (and the 1982 one) are found in the literature with several designations: AzV, AV, AZ, AZO, or AzVi.
Probable SMC Members AzV Number in the catalogue --- RAh Right Ascension 1975 (hours) h RAm Right Ascension 1975 (minutes) min DE- Declination 1975 (sign) --- DEd Declination 1975 (degrees) deg DEm Declination 1975 (minutes) arcmin SpType Spectral Type --- u_SpType Uncertainty flag (:) on SpType --- Vmag Visual Magnitude in Johnson's system, mean error = 0.02mag mag u_Vmag Uncertainty flag (:) on Vmag --- B-V Color in Johnson's system, mean error = 0.015mag mag u_B-V Uncertainty flag (:) on B-V --- U-B Color in Johnson's system, mean error = 0.02mag mag u_U-B Uncertainty flag (:) on U-B --- Obs Number of measurements --- r_Obs An '*' indicates observations by Dachs =1970A&A.....9...95D --- Chart1 Finding Chart Number --- Chart2 Finding Chart Number --- Chart3 Finding Chart Number --- Member "KM" if star already stated as SMC member number=1 "KM" indicates a SMC member by Arp H.C =1958AJ.....63..118A Feast M.W.. et al. =1960MNRAS.121..337F Thackeray A.D. =1962MNSSA..21...74T Sanduleak N. =1968AJ.....73..246S Dachs J. =1970A&A.....9...95D Florsch A. =1972POStr...2....1F --- Rem Remark in the original publication --- CDS Catalogues Service CDS 1995 Nov 08 UNKNOWN UNKNOWN * October 1978: the catalogue was provided as punched cards by M. Azzopardi to CDS. * Description by N.G. Roman [ADC] * 08-Nov-1995: a dedicated column 'r_Obs' was created for the asterisk indicating previous observations Documentation standardized by F. Ochsenbein [CDS] V_13A.xml uvby Estimated Astrophysical Parameters 5014 V/14 uvby Estimated Astrophysical Parameters uvby Estimated Astrophysical Parameters A G D Philip D Egret Astron. Astrophys. Suppl. 40 199 1980 1980A&AS...40..199P Photometry, uvby, beta Observed values of the Stromgren colors were collected from the literature. A computer program calculated the reddening for each star. This value was used to compute the unreddened value of (b-v), c, and m. These were then used to compute [c(1)], [m(1)], and [u-b] for the star. Except for the H beta index, the observed quantities are not included.
The stars were divided into groups by spectral types by means of the bracket quantities. Stars which deviated too greatly from the standard relations could not be dereddened. These include peculiar stars and high luminosity stars and are listed in reject.dat. Various discussions by Crawford were followed to deredden the other stars. The zero point of the [Fe/H] relation was changed from 0.4 to 0.2 on the basis of the study by Gustafsson and Nissen (1972) and some corrections were made to the effective temperature scale in order to fit the new model by Kurucz (1979). Otherwise, the derivations followed the methods of Philip, Miller, and Relyea (1976).
Estimated astrophysical parameter data ID Star Code see nmsys.dat --- (b-y)0 Dereddened Stromgren color: b-y Stromgren Parameters corrected from interstellar reddening mag (c1)0 Dereddened Stromgren c mag (m1)0 Dereddened Stromgren m mag Hbeta Dereddened Stromgren Hbeta mag c1 Derived [c(1)] Stromgren Parameters independent of interstellar extinction mag m1 Derived [m(1)] mag u-b Derived [u-b] mag E(b-y) Derived redenning in (b-y) mag dm1 Deviation from the mean [m(1)] difference between the dereddened parameters of the star and the ZAMS parameters: dm = mz - m0 mag dc1 Deviation from the mean [c(1)] difference between the dereddened parameters of the star and the ZAMS parameters: dc = c0 - cz mag Sp Main Spectral Group for the star Spectral Group: B, A*, A, F, AM, AP --- MK MK Classification of the star MK classification of the star (compiled by Jaschek M., 1979) --- V Derived Absolute V Magnitude mag theta Derived Effective Temperature theta = 5040 / T --- log_g Gravity, derived log(g). cm.s-2 Fe/H Iron/Hydrogen Abundance, derived [Fe/H] a logarithmic difference --- ref Bibliographical References to original data --- Mermilliod numbering system nmsys Mermilliod coded number system Mermilliod J.C. 1973, Rapport interne du CDS 5. --- Julie Anne Watko SSDOO/ADC 1996 Aug 15 V_14.xml SAO and Supplementary Data 5015 V/15 SAO and Supplementary Data SAO and Supplementary Data F Ochsenbein Bull. Inf. CDS 19 74 1980 1980BICDS..19...74O I/131 : SAO Star Catalog J2000 (SAO Staff 1966; USNO, ADC 1990) Ochsenbein, F., Bischoff, M., Egret, D.: 1981, A&AS 43, 265 Jenkins, L.F.: 1952, "General Catalogue of Stellar Trigonometric Parallaxes", Yale Univ. Obs. (see catalog <I/10>) Jenkins, L.F.: 1963, "Supplement to the General Catalogue of Stellar Trigonometric Parallaxes", Yale Univ. Obs. (see catalog <I/81>) Radial velocities Combined data Photometry, UBV MK spectral classification This SAO catalogue (Smithsonian Astrophysical Observatory Catalogue of 258,997 stars, 1966; see catalog <I/131>), connected to the CSI (Catalogue of Stellar Identifications, see Ochsenbein et al. 1981), enables researchers to retrieve reliable astrophysical data for about 20,000 stars. This includes SAO identifications, CSI identifications, equatorial coordinates (B1950), Galactic coordinates, proper motions, photometric data, spectral classifications, radial velocity, etc. The SAO/HD cross index for about 188,000 stars allows users to find (or enter) the catalog with the HD number of the star. The notes contain detected errors, the value of the trigonometric parallax taken from the Jenkins' (1952, 1963) catalogues, the double star designation ADS or IDS, and the name of the star.
The catalog SAO SAO number --- n_SAO a note is detailed in file "notes.dat" --- HD HD number --- m_HD component; / indicates consecutive BD numbers --- DM DM designation DM covers the Bonner, Cordoba and Cape Durchmusterungen designations: when byte 18 blank, DMcode specifies which DM: 0 .. 19 = BD 20 .. 39 = CoD 40 .. 59 = CPD When byte 18 is not blank (contains a dash), the star is not in any Durchmusterung, and DMcode is non-zero for components of multiple systems. --- DMcode DM catalog --- RAh Right ascension - hours (1950.0) h RAm Right ascension - minutes (1950.0) min RAs Right ascension - seconds (1950.0) s DE- Declination sign --- DEd Declination degrees (1950.0) deg DEm Declination minutes (1950.0) arcmin DEs Declination seconds (1950.0) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg pmRA Proper motion in RA arcsec/a q_pmRA Quality of proper motion in RA A = me. <= 0.01"/a B = me. <= 0.02"/a C = me. <= 0.03"/a D = me. <= 0.04"/a E = me. > 0.04"/a --- pmDE Proper motion in DE arcsec/a q_pmDE Quality of proper motion in DE --- Mag Generally V magnitude, sometimes B From Nicolet if available (1978a); otherwise from Blanco et al. (1968) improved by Ochsenbein (1974) mag q_Mag Quality of/note on magnitude : only a CSI magnitude with 0.1 magnitude precision ** indicates that Mag contains a blue magnitude Quality index from compilation of UBV by Nicolet: A = very good (4 in original catalog) to D = poor (1 in original catalog) --- B-V B-V color mag q_B-V Quality of B-V Quality index from Nicolet compilation: A = very good (4 in original catalog) to D = poor (1 in original catalog) --- U-B U-B color mag q_U-B Quality of U-B --- q_Sp Quality of spectral type J = from Jaschek (1978, see catalog <III/42>) 1 to 4 = Quality from Michigan Catalog (N. Houk, 1975, 1978. see catalogues <III/31> and <III/51>) where 1 is optimum and 4 is very poor blank = from CSI --- per Period (punctuation) --- Sp Spectral type --- RV Radial Velocity Taken, as available in the following order: the "Catalogue of Stellar Radial Velocities" by Evans (1967 ) (see catalog <III/47>) the "General Catalogue of Stellar Radial Velocities" by Wilson (1953) (catalog <III/21>) the "Bibliographic Catalogue of Radial Velocities" by Barbier (1975) the "Bibliography of Stellar Radial Velocities" by Abt et al. (1972) (catalog <III/4>) km/s q_RV Quality on radial velocity Quality index as in Wilson (catalog <III/21>), i.e. A good (p.e. <= 0.9km/s) B (p.e. <= 2km/s) C (p.e. <= 5km/s) D poor (p.e. <= 10km/s) --- Cross index of SAO numbers in HD order HD_cat Catalog acronym --- HD HD number --- m_HD HD component (in multiple systems) --- SAO_cat Catalog acronym --- SAO SAO number --- Remarks for SAO 1 - 99999 SAO SAO number --- Text Text of remark --- N.G. Roman ADC/SSDOO 1997 Sep 12 V_15.xml A list of stars classified as Supergiants 5017A V/17A A list of Supergiant Stars A list of stars classified as Supergiants D Egret Bull. Inform. CDS 18 82 1980 1980BICDS..18...82E Stars, supergiant This catalogue is a compilation of about 5000 stars classified as supergiants (class I or II) in the literature. The following information is given: DM and HD identifications, coordinates, photometry, radial velocity and MK classification
The list of Supergiants CSI designation number=1 The CSI designation (see Ochsenbein et al. 1980) is made of 3 parts: the zone, the number, and a code. For a positive number, the code indicates which Durchmusterung the zone and number refer to: - BD (Bonner Durchmusterung) for 0 <= code <= 19 - CD (Cordoba Durchmusterung) for 20 <= code <= 39 - CPD (Cape Durchmusterung) for 40 <= code <= 59 A negative number (constructed from 1950 right ascension) is assigned for non-DM stars. --- HD Henry Draper Catalogue Designation --- m_HD Multiplicity index on HD number; a '/' indicates a group of 2 HD numbers --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s u_RAs for poor position (accuracy 1arcmin) --- DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg n_Vmag Variability or Duplicity indicator --- Vmag Visual magnitude mag u_Vmag Uncertainty flag (:) on Vmag --- q_Vmag Quality indicator on Vmag number=2 the quality number (1=poor, 4=good) comes from the UBV catalogue by Nicolet (1978); --- B-V Colour mag q_B-V Quality indicator on B-V number=2 the quality number (1=poor, 4=good) comes from the UBV catalogue by Nicolet (1978); --- U-B Colour mag q_U-B Quality indicator on U-B number=2 the quality number (1=poor, 4=good) comes from the UBV catalogue by Nicolet (1978); --- Gflag 'G' when Geneva photometry exists --- Uflag 'U' when uvby photometry exists --- RVel Radial Velocity from Wilson (1953) or Evans (1967) km/s q_RVel Quality on Radial Velocity (A=good, E=very poor) --- n_Sp Dispersive system used, or quality from Houk's catalogue (when Sep='X') number=3 The MK classification from N. Houk (1975, 1978) includes a quality from 1 (good) to 4 (poor), a '+' for spectra classified in other sources, and 'X' when several spectra were available. When Sep is a '/', the classification is from Jaschek (1978) --- Sep Separator ('X' when Sp is from Houk) --- Sp Spectral classification number=3 The MK classification from N. Houk (1975, 1978) includes a quality from 1 (good) to 4 (poor), a '+' for spectra classified in other sources, and 'X' when several spectra were available. When Sep is a '/', the classification is from Jaschek (1978) --- Francois Ochsenbein CDS 1995 Jul 12 UNKNOWN UNKNOWN * June 1980: catalogue prepared and archived at CDS * 12-Jul-1995: the catalogue was reformatted at CDS: => elimination of record headers "5017A1" => creation of a dedicated column for the ':' uncertainty flag u_Vmag which was previously embedded in the Vmag column => addition of the standard documentation V_17A.xml Catalogue of Late-type Stars with OH, H2O or SiO Maser Emission 5018 V/18 Catalogue of Late-type Stars with Maser Emission Catalogue of Late-type Stars with OH, H2O or SiO Maser Emission D Engels Astron. Astrophys. Suppl. Ser. 36 337 1979 1979A&AS...36..337E V/68 : Catalog of observations for stellar masers (Benson+ 1990) Masers Stars, late-type Stars, masers Stars, radio A catalog of more than 300 late type stars which display maser line radio emission in OH, H2O or SiO molecules has been compiled. About two thirds of the objects have been identified with optical or infrared optics, mostly M-supergiants, Mira, or semiregular variables. The catalog contains optical data such as spectral type, period and magnitude, radio flux densities and velocities and infrared flux densities in the region between 0.7 and 20 micrometers.
The systematic literature search is complete up to January 1, 1979. The catalogue ends with a reference list containing all objects followed by a code number and a list containing the literature belonging to each code number. The literature cited for each object contains all data used, except data from the general catalogue of variable stars, the two-micron sky survey and the AFCRL infrared sky survey. See the source reference for additional information. The catalogued stars are divided in six groups M-supergiant stars Type I OH/IR stars Type II OH/IR stars H2O/IR stars without detected OH-emission SiO/IR stars Objects undetected in the optical or infrared
Optical and infrared data type Type of star number=1 M = M-supergiant stars IR = Type I OH/IR stars IRII = Type II OH/IR stars H2O = H2O/IR stars without detected oh-emission SiO = SiO/IR stars --- ID Designation of star --- name Alternative designation(2) --- RAh Right Ascension hours (1950) h RAm Right Ascension minutes (1950) min RAs Right Ascension seconds (1950) s DE- Declination sign --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin dist Distance number=3 Generally from the Catalogue of Variable Stars (see cat. <II/139>) or from the cited literature at the end of the catalogue pc VarType Type of variable number=3 Generally from the Catalogue of Variable Stars (see cat. <II/139>) or from the cited literature at the end of the catalogue --- MaxMag Maximum magnitude number=3 Generally from the Catalogue of Variable Stars (see cat. <II/139>) or from the cited literature at the end of the catalogue mag l_MinMag Note on following magnitude number=7 "(" Signifies that the variable at minimum can be fainter than the magnitude given after this symbol "V" Denotes photoelectrical measurement --- MinMag Minimum magnitude number=3 Generally from the Catalogue of Variable Stars (see cat. <II/139>) or from the cited literature at the end of the catalogue mag Imag I magnitude from Two Micron Survey mag Kmag K magnitude from Two Micron Survey mag I(1.04) I(1.04um) on Lockwood and Wing system (1971ApJ...169...63L) W/cm2/um R-flux Flux near wavelength = 0.7 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um I-flux Flux near wavelength = 0.9 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um J-flux Flux near wavelength = 1.25 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um H-flux Flux central wavelength = 1.65 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um K-flux Flux at near wavelength = 2.25 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um L-flux Flux near wavelength = 3.5 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um M-flux Flux near wavelength = 4.9 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um flux-8 Flux near wavelength = 8.55 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um N-flux Flux near wavelength = 10.1 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um flux-11 Flux near wavelength = 10.95 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um Q-flux Flux near wavelength = 19.75 um number=4 Negative logarithmic flux densities in W/cm^2/um W/cm2/um cal Key to calibration system number=5 The flux densities were computed from the colors using the calibrations referenced in cal as follows: 1 = Johnson (1966, Ann. Rev. Astron. Astrophys. 4, 193) and Dyck et al. (1974ApJ...189...89D) 2 = Hyland et al. (1972A&A....16..204H) 3 = Wilson et al. (1972ApJ...177..523W) 4 = Gillet et al. (1971ApJ...164...83G) 5 = Schultz et al. (1976A&A....50..171S) 6 = Beckwith et al. (1976ApJ...208..390B) 7 = Strecker and Ney (1974AJ.....79..797S) --- Sp Spectral type number=3 Generally from the Catalogue of Variable Stars (see cat. <II/139>) or from the cited literature at the end of the catalogue --- P Period of variation number=3 Generally from the Catalogue of Variable Stars (see cat. <II/139>) or from the cited literature at the end of the catalogue d rem Notes on individual stars number=6 (1) = NML Cyg (2) = P.F. Bowers detected three OH-peaks (86) (3) = Third OH-peak at 2 km/s detected (19) (4) = OH/IR classification uncertain (5) = Third OH-peak at -28 km/s detected (44) (6) = = OH 320.7+3.4, optical identification uncertain (39) (7) = Complex H2O-spectrum (88) (8) = Tw peg is probably a SR-type supergiant (9) = Possible opt.id. by Lebofsky,M.J.,Kleinmann,S.G. (1976AJ.....81..534L) (10) = Coincidence of radio- and infrared-emission source not confirmed (11) = Probably CRL 2188 --- Seq Running number of star --- OH and H2O data Type Type of star --- ID Designation of star number=1 Several records may concern the same star --- name Alternative designation number=1 Several records may concern the same star --- f1_1612 OH flux at 1612 MHz first component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v1_1612 LSR velocity of 1st comp. at 1612 MHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f2_1612 OH flux at 1612 MHz 2nd component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v2_1612 LSR velocity of 2nd comp. at 1612 MHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f1_65/7 OH flux at 1665/67 MHz 1st comp. number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v1_65/7 LSR velocity of 1st comp. at 1665/67MHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f2_65/7 OH flux at 1665/67 MHz 2nd comp. number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v2_65/7 LSR velocity of 2nd comp. at 1665/67MHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s H2O_flux H2O flux for the principal feature number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy H2O_vel H2O LSR velocity for the principal feature km/s SiO SiO presence indicator number=3 + = object is listed in SiO.dat - = no SiO was found --- Seq Running number number=1 Several records may concern the same star --- Data for SiO masers ID Designation of star --- name Alternative designation --- f1_43 SiO flux at 43 GHz 1st component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v1_43 Velocity of 1st component at 43 GHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f2_43 SiO flux at 43 GHz 2nd component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v2_43 Velocity of 2nd comp. at 43 GHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f1_86 SiO flux at 86 GHz 1st component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v1_86 Velocity of 1st comp. at 86 GHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f2_86 SiO flux at 86 GHz 2nd component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v2_86 Velocity of 2nd comp. at 86 GHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s fa_43 SiO flux at 43 GHz additional component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy va_43 Velocity of additional comp. at 43 GHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s Seq Running number --- Radio data for stars not detected in the infrared or optical regions ID Identification of star number=1 Star 316 has two lines of data. --- RAh Right Ascension hours (1950) h RAm Right Ascension minutes (1950) min RAs Right Ascension seconds (1950) s DE- Declination sign --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin f1_1612 OH flux at 1612 MHz 1st component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v1_1612 Velocity of 1st component at 1612 MHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f2_1612 OH flux at 1612 MHz 2nd component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v2_1612 Velocity of 2nd comp. at 1612 MHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f1_65/7 OH flux at 1665/67 MHz 1st component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v1_65/7 Velocity of 1st comp. at 1665/67 MHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s f2_65/7 OH flux at 1665/67 MHz 2nd component number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. Jy v2_65/7 Velocity of 2nd comp. at 1665/67 MHz number=2 In the original catalog some fields contain ---, some contain det, and some are blank. The --- and det indicate no detection or missing data but the paper gives no explanation as to how these values differ or how either differs from blank. In view of this, they have been removed. these entries differ from blank fields or from each other. km/s H2O_flux H2O flux at 22GHz for principal feature Jy H2O_vel H2O velocity at 22GHz for the principal feature km/s SiO SiO presence indicator number=3 + = object is listed in SiO.dat - = no SiO was found --- rem Remark number=4 1 = Previous name: 1647-41 2 = Previous name: 1735-32 3 = Previous name: 1821-12 4 = Previous name: W41 5 = OH/IR classification uncertain 6 = Previous name: 1837-05 7 = Previous name: W43A 8 = Probably CRL 2403 (95) 9 = At 1665 MHz peak at 11 km/sec 10 = Previous name: ON-4 --- Seq Running number number=1 Star 316 has two lines of data. --- References to the data for each star Seq Running number of star number= References in parentheses contain further IR data --- name Name number= References in parentheses contain further IR data --- codes Codes of references containing star References in parentheses contain further IR data number= References in parentheses contain further IR data --- Key to reference numbers in biblio.dat code Code number The field is repeated for continuation lines number= The field is repeated for continuation lines number= AP.J. = Astrophysical Journal AP.LETTERS = Astrophysical Letters ASTR.J. = Astronomical Journal ASTR.AP. = Astronomy and Astrophysics BOL.OBS.T.T. = Boletin de los Observatorios Tonanzintla y Tacubaya MNRAS = Monthly Notices of the Royal Astronomical Society NAT. = Nature PASP = Publications of the Astronomical Society of the Pacific --- text Corresponding reference AP.J. = Astrophysical Journal AP.LETTERS = Astrophysical Letters ASTR.J. = Astronomical Journal ASTR.AP. = Astronomy and Astrophysics BOL.OBS.T.T. = Boletin de los Observatorios Tonanzintla y Tacubaya MNRAS = Monthly Notices of the Royal Astronomical Society NAT. = Nature PASP = Publications of the Astronomical Society of the Pacific number= The field is repeated for continuation lines number= AP.J. = Astrophysical Journal AP.LETTERS = Astrophysical Letters ASTR.J. = Astronomical Journal ASTR.AP. = Astronomy and Astrophysics BOL.OBS.T.T. = Boletin de los Observatorios Tonanzintla y Tacubaya MNRAS = Monthly Notices of the Royal Astronomical Society NAT. = Nature PASP = Publications of the Astronomical Society of the Pacific --- Nancy Grace Roman SSDOO/ADC F. Ochsenbein CDS 1995 Dec 28 V_18.xml Catalog of Masses and Ages of Stars in 68 Open Clusters 5019 V/19 Masses and Ages of Stars in 68 Open Clusters Catalog of Masses and Ages of Stars in 68 Open Clusters A Piskunov CDS Bull. No. 19, p. 67 ??? ??? 1980 1980BICDS..19...67P Clusters, open Stars, ages Stars, masses This catalog contains the evolutionary masses and ages of about 7000 stars in 68 open clusters. Cluster ages range from 10**6 to some 10**9 years, and their population varies from 30 to 700 members. For each cluster we have a table with ages and masses of stars. The file, clusters.dat may include for each cluster, the name (or NGC/IC number), cluster class, assumed color index E(B-V), true distance modulus (V-M_V)_0, evolutionary tracks used for given cluster and reference to the source of UBV data. The data in data.dat consists of star serial number, color index, V magnitude, luminosity, effective temperature, and ages and masses of stars.
Data for individual stars Cl Cluster number. for name see clusters.dat If blank, then same as previous. Cl is only listed for first record of cluster. Fields N through L are only listed for first record of star. --- N Running number for each cluster --- ID Star number in UBV source --- B-V B-V color index mag V V magnitude mag LC Adopted luminosity class --- Teff Logarithm effective temperature --- L Logarithm of luminosity --- Age Age of the star For stars lying under the ZAMS or to the right of the Hayashi limit, ages are formally defined and are negative, but have no physical meaning. Some stars lie in the forbidden regions of the H-R diagram due to errors of photometry, of conversion procedure, etc. To these stars, reasonable values of age and mass cannot be attributed. In this case, zeros appear in the Age, Mass and Prob fields. a Mass Mass of the star solMass Prob Probability in percent --- General information on each cluster text Text of header for cluster --- Julie Anne Watko SSDOO/ADC 1997 Jan 08 V_19.xml CSI Catalogue with Selected Data 5026 V/26 CSI Cat with Selected Data CSI Catalogue with Selected Data F Ochsenbein CDS Inf. Bull. No. 24, p. 109 ??? ??? 1983 1983 Combined data Photometry, UBV Proper motions Radial velocities This catalogue contains the stars of the Catalogue of Stellar Identifications (CSI, see e.g. Ochsenbein, Bischoff, Egret 1981). For these 434023 stars, positions, proper motions, radial velocities, UBV photometry, and the spectral classification are listed. The absolute magnitude was computed from these data using the methods described by Ochsenbein and Egret (1981) for the "Preparation of a list of stars expected to be nearer than 200 pc"
Catalogue CSIzone CSI identifier zone --- CSInum CSI identifier number --- CSIcat CSI identifier catalog code 0-19 for BD 20-39 for CoD >=40 for CPD --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin GLON Galactic longitude deg GLAT Galactic latitude deg Mv Absolute magnitude mag n_Mv Method used to derive Mv A to F: from Gliese's "Catalogue of Nearby Stars" (1969) G: derived from MK spectral type H: derived from HD spectral type and proper motions (Ochsenbein and Egret, 1981) --- Av Absorption computed from E(B-V) mag n_Av Method used to derive Av always F = derived from Photometry --- r_Sp Origin of Spectral Type J = Selected by Jaschek (1978) H = Spectrum from "Michigan Spectral Survey" (Houck, 1975, 1978) --- Sp Spectral classification --- Tcode Temperature class code Coding of Temperature Class ---------- ---------- ---------- ---------- ----------- 004 O5 058 B8.5 114 F4 174 K3.5 225 WN 008 O6 060 B9 116 F5 176 K4 226 WR 010 O6.5 061 B9.2 118 F5.5 178 K4.5 227 WC 012 O7 062 B9.5 120 F6 180 K5 228 O 014 O7.5 063 B9.7 122 F6.5 181 K6 229 B 016 O8 064 A0 124 F7 182 K7 230 A 018 O8.5 066 A0.5 126 F7.5 183 K8 231 F 020 O9 068 A1 128 F8 184 M0 232 G 021 O9.2 070 A1.5 130 F9 186 M0.5 233 K 022 O9.5 072 A2 132 G0 188 M1 234 M 023 O9.7 074 A2.5 134 G0 5 190 M1.5 235 R 024 B0 076 A3 136 G1 192 M2 236 N 025 B0.2 078 A3.5 138 G1 194 M2.5 237 S 026 B0.5 080 A4 140 G2 196 M3 238 C 027 B0.7 082 A4.5 142 G2.5 198 M3.5 239 C comp. 028 B1 084 A5 144 G3 200 M4 241 WN comp. 030 B1.5 086 A5.5 146 G4 202 M4.5 242 WR comp. 032 B2 088 A6 148 G5 204 M5 243 WC comp. 034 B2.5 090 A6.5 150 G5.5 206 M5.5 244 O comp. 036 B3 092 A7 152 G6 208 M6 245 B comp. 038 B3.5 094 A7.5 154 G7 210 M6.5 246 A comp. 040 B4 096 A8 156 G8 212 M7 247 F comp. 042 B4.5 098 A8.5 158 G9 214 M7.5 248 G comp. 044 B5 100 A9 160 K0 216 M8 249 K comp. 046 B5.5 102 A9.5 162 K0.5 250 M comp. 048 B6 104 F0 164 K1 251 R comp. 050 B6.5 106 F1 166 K1.5 252 N comp. 052 B7 108 F2 168 K2 253 S comp. 054 B7.5 110 F2.5 170 K2.5 254 Comp? 056 B8 112 F3 172 K3 255 ??? ---------- ---------- ---------- ---------- --- Dot1 '.' --- Lcode Luminosity class code Coding of Luminosity Class ---------- ---------- ---------- ----------- 00 Unknown 10 Ib-II 15 IIIa 22 IV-V 02 Ia-0 11 IIa 16 III 24 V 04 Ia 12 II 17 IIIb 28 VI (sd) 06 Iab 13 IIb 18 III-IV 08 Ib 14 II-III 20 IV ---------- ---------- ---------- --- Dot2 '.' --- Sp_v 1 for Variable spectrum --- Sp_e 1 for Emission spectrum --- Sp_sh 1 for Shell spectrum --- Sp_p 1 for Peculiar spectrum --- Sp_Prof Code for nebulosity 1 for sharp lines (s), 2 for nebulous lines (n), 3 for very nebulous lines (nn) --- Sp_El Code for elements 1 for CN-pec (CN) 2 for weak-line (w) 3 for metallic-line (m) --- r_V Reference code for photometry 'F' for photoelectric UBV (Mermilliod and Nicolet, 1977) 'Y' when photometric indices derived from homogenized magnitudes (Ochsenbein, 1974) 'B' when only B magnitude is known --- V V magnitude, or B magnitude if r_Phot = 'B' mag q_V Quality index from A (very good) to D (poor) --- (B-V) (B-V) color index mag q_(B-V) Quality index from A (very good) to D (poor) --- (U-B) (U-B) color index mag q_(U-B) Quality index from A (very good) to D (poor) --- n_V Notes on Photometry: D=Double, V=Variable --- r_pmRA Origin of pmRA and pmDE A = AGK3 S = SAO C = CPC Y = Yale --- pmRA Proper motion in RA (mult. by cos(Dec)) mas/a e_pmRA Mean error on pmRA mas/a pmDE Proper motion in Declination mas/a e_pmDE Mean error on pmDE mas/a RV Radial velocity, mainly from Wilson (1953) km/s q_RV Quality index from A (very good) to E (poor) --- Francois Ochsenbein CDS J.A. Watko SSDOO/ADC 1996 Jul 15 V_26.xml Proper Motions and UBV Photometry of Stars in the Region of the h and Chi Persei Clusters 5027 V/27 Proper Motions, UBV Photometry, Region of h,Chi Per Proper Motions and UBV Photometry of Stars in the Region of the h and Chi Persei Clusters M Muminov Astron. Inst. Acad. Sci. uzb.SSR, Tashkent, unpublished ??? ??? 1980 1980 Clusters, open Proper motions Photometry, UBV Associations, stellar Regional catalog Proper motions with an 80 year baseline have been determined relative to reference stars with B=13.9mag. determined for 3086 stars brighter than B=15.5mag. within an area of 50' radius, centered at RA = 2h16.9m, Dec = +57d0.1' (1950.0). Proper motions were also measured for 1055 stars with 15.5 le B le 17.1 mag. in two areas 14' in radius, centered on the h and chi Persei clusters. Proper motions are also given for 1386 stars in an adjacent area (RA = 2h06.7m; Dec = +56d57')for 1386 stars with a 38 year baseline.
The mean errors of the proper motions are equal in right ascension and declination. For the h and chi Perseus region, they are 0.0021"/a and for the adjacent region, they are 0.0031"/a. The proper motions in the adjacent area have been reduced to the system of those in the cluster region using 214 stars in common. The number of measured plates measured for magnitudes and the corresponding errors are given in the following table: FILE NAME # PLATES ERRORS (10-2arcsec/a) V B U V B U ----------------------------------------------------- data1.dat 2 3 2 6 5 6 data2.dat 1 2 - 8 6 - adjarea.dat 2 2 2 6 6 6 _____________________________________________________
B < 15.5 mag ID Star number --- X X-coordinate mm Y Y-coordinate mm V V magnitude m B-V B-V color index m U-B U-B color index m pmX X-Annual proper motion 10-4arcmin/a pmY Y-Annual proper motion 10-4arcmin/a prob Cluster membership probability based on proper motions and photometry. % Cl_mem Cluster membership * = member of the cluster. --- AGK3zone AGK 3 zone --- dash separator --- AGK3num AGK 3 number --- B > 15.5 mag ID Star number --- X X-coordinate mm Y Y-coordinate mm V V magnitude mag B-V B-V color index mag pmX X-Annual proper motion 10-4arcmin/a pmY Y-Annual proper motion 10-4arcmin/a prob Cluster membership probability based on proper motions and photometry. % Cl_mem Cluster Membership * = member of the cluster. --- MVzone Moffat and Vogt zone --- dash separator --- MVnum Moffar and Vogt number --- Adjacent Area ID Star number --- X X-coordinate mm Y Y-coordinate mm V V magnitude mag B-V B-V color index mag U-B U-B color index mag pmX X-Annual proper motion 10-4arcmin/a pmY Y-Annual proper motion 10-4arcmin/a AGK3z AGK3 zone --- dash separator --- AGK3no AGK3 number --- Julie Anne Watko SSDOO/ADC 1996 Apr 08 V_27.xml Proper Motions and UBV Photometry of Stars in the Region of Open Clusters NGC 7788, NGC 7790, Berkeley 58 and Anonymous 5028 V/28 Proper Motions, UBV Photometry, Four Open Clusters Proper Motions and UBV Photometry of Stars in the Region of Open Clusters NGC 7788, NGC 7790, Berkeley 58 and Anonymous V N Frolov Pulkovo Obs., unpublished ??? ??? 1980 1980 Clusters, open Proper motions Photometry, UBV Regional catalog Proper motions were determined for 2169 stars with limiting magnitude B = 16.5 mag and located within a 60 x 60 area centered at RA = 23 h 54.2 min, Dec = 60 deg 57 arcmin (1950.0). Three plate pairs with a mean epoch difference of 49 years were used. The first epoch plates were taken with the Tashkent normal astrograph during 1923-1925 and the second epoch plates with the Pulkovo normal astrograph. The proper motions have a mean error +/-0.0030 arcsec (B < 14.5 mag) and +/-0.0036 arcsec (B > 14.5 mag) and were measured relative to reference stars with 13.5 mag <= B <= 14.5 mag. Photographic UBV magnitudes were measured using Sandages photoelectric standards. The U, B and V magnitudes were determined for 1930, 2165 and 1734 stars respectively, with the corresponding mean errors +/-0.03 mag, +/-0.06 mag and +/-0.05 mag. In the measured area there are three known open clusters (NGC 7788, NGC 7790 and Berkeley 58) and a previously unknown open cluster, discovered by the author, centered at RA =23 h 54.9 min, Dec = 61 deg 21 arcmin (1950.0). The cluster members were selected on the basis of the proper motion (vector diagram) and photometric (V ~ B-V and U-B ~ B-V) criteria. Stars within areas with 4 arcmin radii centered on NGC 7788 and NGC 7790 and 6 arcmin radii centered on Berkeley 58 and the anonymous cluster were investigated for cluster membership. The method of reduction of the observational data and the results obtained have been published in Izv. Pulkovo 195, 80, 1977 and 196, 69, 1979.
Photometry and Proper Motions Data ID Star Number --- X X-Coordinate mm Y Y-Coordinate mm V V Magnitude The following stars are known variables 327 - Cepheid CG Cas 693 - Algol Type Variable 893 - Double Cepheid CE Cas 903 - Cepheid CF Cas mag B-V B-V color index mag U-B U-B color index mag pmX X-annual proper motion 10-4arcmin/a pmY Y-annual proper motion 10-4arcmin/a Cl_mem Cluster Membership Cluster Membership Designation 7788 = member of NGC 7788 7790 = member of NGC 7790 58 = member of Berkeley 58 1 = member of anonymous cluster 0 = no designation --- Julie Anne Watko SSDOO/ADC 1996 May 30 V_28.xml Catalogue of Kinematic Data for O-B5 stars 5031A V/31A Kinematic data for O-B5 stars Catalogue of Kinematic Data for O-B5 stars V C Rubin J Burley A Kiasatpoor B Klock G Pease E Rutscheidt C Smith Astron. J. 67 491 1962 1962AJ.....67..491R Stars, early-type Stars, OB This document describes the magnetic tape version of a catalog of 1440 O-B5 star with radial velocities accurate to within 5 km/sec, located within 3 kpc of the sun and within 10 degrees of the galactic equator. Radial velocities, luminosities and spectral classifications have been included from the literature; proper motions have been compiled for 898 of the stars.
The catalogue Num Running number --- pmPubl "*" if star has a published proper motion --- r_RVel Source for radial velocity if not in GCRV (see "refs" file) --- GCRV GCRV (Wilson ref. 58) number --- HD Henry Draper (HD) Catalogue number --- Other Identifier if no HD number was available number=1 If no HD number is available, this designation represents depending on byte 22: "+" or "-" : sign of Bonner Durchmusterung (BD) or Cape Photographic Durchmusterung (CPD) For BD and CPD numbers, form is ZZNNNNNL where ZZ = absolute value of declination zone NNNNN = number within zone L = blank, or "A", "B", etc. "A" : Aitken Double Star Catalogue number "I" : Index Catalogue (IC) number "K" : Rspteyn (K) Selected Area number "M" : Messier's (M) Catalogue number "N" : New General Catalogue (NGC) number --- Gl Galactic longitude 0.01deg Gb Galactic latitude 0.01deg RAh Right ascension in hours [B1950] h RAdm Right ascension in tenths of minutes [B1950] 0.1min DE- Sign of declination --- DEd Declination degrees [B1950] deg DEm Declination arcminutes [B1950] arcmin RVel Radial velocity km/s Vmag Visual or Photographic magnitude (see n_Vmag) mag n_Vmag Remark on Vmag number=2 the following remark concerns the magnitude: "P" indicates a photographic magnitude; "V" refers to a variable; "+" indicates a variable photographic ":" indicates last digit is uncertain --- Sp Spectral classification, on the MK system when available --- AbsMag Absolute magnitude (M) when available, most often from Johnson and Iriarte (1958, ref.25) 0.1mag n_AbsMag The "*" indicates stars with no luminosity class available; class V was assumed and Johnson-Iriarte calibration adopted --- Av Visual absorption (Av) number=3 the absorption is most often from (B-V) measures. A value of 3 for the ratio of total to selective absorption has been assumed. The entry Av = 0.0 indicates that the computed value was negative, but always equal to 0.0 to one decimal place. mag m-M Distance modulus computed from m-M-Av 0.1mag n_m-M "*" indicates that photometric data were missing for second star in a binary --- r_Vmag Source for visual apparent magnitude Vmag --- r_Sp Source for spectral classification --- r_AbsMag Source for absolute magnitude M --- r_Av Source for visual absorption Av --- pmRA Proper motion in right ascension 0.1ms/yr pmDE Proper motion in declination mas/yr pmGLON Proper-motion in galactic longitude mas/yr pmGLAT Proper-motion in galactic latitude mas/yr r Heliocentric Distance computed from (m-M) 100pc R Galactocentric distance (Rsun=8.2kpc) 100pc Tl Tangential motion in galactic frame number=4 velocity not corrected for the solar motion km/s Tb Tangential motion in galactic frame number=4 velocity not corrected for the solar motion km/s xdot Space motion of the star number=4 velocity not corrected for the solar motion km/s ydot Space motion of the star number=4 velocity not corrected for the solar motion km/s zdot Space motion of the star number=4 velocity not corrected for the solar motion km/s cirVel Circular velocity (ortho-radial in the galactocentric frame) km/s e_cirVel Probable error on cirVel km/s Pi Radial velocity in the galactocentric frame km/s e_Pi Probable error on Pi km/s pmRef References for proper motions number=5 References of proper motions: --------------------------------------------------------------------- Number Prob.Err. # Stars (mas/yr) --------------------------------------------------------------------- 1 Bertiau, F. C., S. J. 1958 30 3 Astrophys. J., 128, 533. 2 Morgan, H. R. 1956, Astron. J., 61, 90. 304 3 3 Morgan, H. R. 1952, Astron. Papers Am. 51 3 Ephemeris and Naut. Almanac XIII, part III. 4 Trans. Astron. Obs. Yale University, 78 4 24, 1953; 25, 1954; 26, 1959; 27, 1959. 5 Annals Cape Observatory, XVII, 1954; 35 7 XVIII, 1954; XIX, 1958; XX, 1958. 6 Boss, B. 1937, General Catalogue of 211 6 33 342 Stars for Epoch 1950 (Carnegie Institution of Washington, Washington, D.C.) 7 Trans. Astron. Obs. Yale University, 185 7 12, 1940; 13, 1943; 14, 1943; 16, 1945; 17, 1945; 18, 1947; 19, 1948; 20, 1949; 21, 1950; 22, 1950. 8 Reiz, A., 1957, Ann. Lund Obs. 14,1 3 6 9 Morgan, H.R., 1933, Publ. U.S. Naval Obs. 1 6 2nd Ser. XIII, 163. --------------------------------------------------------------------- --- Joseph Florsch CDS 1995 Feb 13 UNKNOWN UNKNOWN * September 1981 (Jaylee M. Mead, Robert S. Hill, ADC): The magnetic tape version of this catalog was obtained from the Centre de Donnees Stellaires (CDS), Strasbourg; it differed from the original catalog in that the spectral type and source references for the apparent magnitude, spectral type, absolute magnitude, absorption and proper motion were omitted. To facilitate processing of the data by computer, we have done the following: 1. Restored the spectral type and all source references 2. Combined Tables I and IV of the published catalog by adding the data for the 898 proper motion stars from Table IV to the appropriate entry in Table I, as indicated by the asterisk in Table I immediately following the running star number. The only entries omitted in the combined table were those which were duplicated in Table IV: star number, galactic longitude and radial velocity. 3. Separated out the Henry Draper Catalog numbers into one field with all other identifiers in the next field; also, separated radial velocity references into a separate field from the GCRV numbers. 4. Filled blank M, Av, and (m-M) fields with nines. * 14-Feb-1995 (J.Florsch and F.Ochsenbein, CDS): => inserted the decimal point in columns RVel, Vmag and Av to avoid any misinterpretation of missing decimals => corrected individual record 105 = HD 169271 V_31A.xml Catalogue of Stars within 25 Parsecs of the Sun 5032A V/32A Stars within 25 pc of the Sun Catalogue of Stars within 25 Parsecs of the Sun R V D R Woolley E A Epps M J Penston S B Pocock Royal Obs. Ann. 5 ??? ??? 1970 1970ROAn....5....1W V/70 : Nearby Stars 3, Preliminary (Gliese, Jahreiss 1991) Gliese, W. 1957, "Katalog der Sterne naher als 20 Parsek fuer 1950.0", Astron. Rechen-Inst. Heidelb., Mitt. A, Nr. 8 Jenkins, L.F. 1952, General Catalogue of Trigonometric Stellar Parallaxes (New Haven; Yale University Observatory) Jenkins, L.F. 1963, Supplement to the General Catalogue of Trigonometric Stellar Parallaxes (New Haven; Yale University Observatory) Wilson, R.E. 1953, General Catalogue of Stellar Radial Velocities, Publ. Carnegie Inst., Washington, No. 601 Stars, nearby This catalog was constructed at the Royal Greenwich Observatory in order to enlarge the Gliese (1957) compilation. It contains data on stars nearer than 25 pc that are not included in Gliese's catalog, plus additional information published since 1957 on stars in the Gliese catalog. The machine version contains essentially all information given in Table Ia of the published catalog, plus positional data, and most cross references to other catalogs given in Table IIa. The notes flags in Table Ia are not included because the notes are not machine-readable. Omitted from Table IIa are the finding-chart indicators (Lowell G numbers or notes references) and miscellaneous cross identifications to other names and catalog identifiers. Tables Ib and IIb, containing 21 systems originally included in Gliese's (1957) catalog but for which revised parallaxes have placed them farther than 25 pc are not included in the machine version. Data in the machine version are Gliese number (Newly added stars begin with 9001, but new parallaxes have removed 9419 and added 9849 and 9850; the Sun [first record] has number 0); component identifications for multiple systems; parallax; annual proper motions; radial velocity; (U,V,W) space velocities; box orbit parameters (omega, e, i); spectral type; UBV data; absolute visual magnitude; right ascension (B1950) declination, GCTP (Jenkins 1952, 1963); HD DM, GCRV (Wilson 1953) and other catalog identifiers; BS (= HR) (Hoffleit 1964) numbers; and remarks codes for SB, doubles, variables, etc. Please note that the first entry is for the Sun, and thus it lacks fields such as RA and Dec.
The catalogue of stars within 25pc Woolley Sequence number Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- m_Woolley Component identification number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- plx Parallax number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. mas e_plx Probable error in plx "S" indicates spectroscopic parallax number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. mas n_plx Note:'8' if e_plx < 15%, '9' if e_plx < 10% number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- pmRA Proper motion in RA number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. s/yr pmDE Proper motion in Dec number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. arcsec/yr RVel Radial velocity number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. km/s n_RVel Note on RV J = combined components of binary V = variable velocity number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- U U component of space velocity (toward galactic centre) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. km/s V V component of space velocity (toward galactic rotation) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. km/s W W component of space velocity (toward North galactic pole) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. km/s GCdist Galactocentric distance in units of Sun's distance from the center i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. 10-4 e Box orbit eccentricity number=1 see details in file "adc.doc" or in the original publication. --- i Box orbit angle (highest inclination of the orbit) number=1 see details in file "adc.doc" or in the original publication. 10-4rad LC_Code Luminosity class code 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- SpType Spectral type number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- r_SpType Coded source of spectral type 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- Mag Magnitude m(v) or m(pg) (see n_Mag) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. mag n_Mag Magnitude code J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- B-V B-V color number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. mag U-B U-B color number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. mag Mv Absolute visual magnitude Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. mag RA1900h Hours RA, equinox B1900, epoch 1900.0 number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. h RA1900dm Minutes RA, equinox B1900, epoch 1900.0 number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. 0.1min DE1900- Sign Dec, equinox B1900, epoch 1900.0 number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- DE1900d Degrees Dec, equinox B1900, epoch 1900.0 number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. deg DE1900m Minutes Dec, equinox B1900, epoch 1900.0 number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. arcmin RAh Right Ascension B1950, epoch 1950 (hours) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. h RAm Right Ascension B1950, epoch 1950 (minutes) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. min RAs Right Ascension B1950, epoch 1950 (seconds) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. s DE- Declination B1950, epoch 1950 (sign) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- DEd Declination B1950, epoch 1950 (degrees) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. deg DEdm Declination B1950, epoch 1950 (deci-minutes) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. 0.1arcmin GCTP Gen. Cat. of Trigonometric Parallaxes <I/60> number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- HD Henry Draper Catalog (HD) number number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- DM Durchmusterung (BD, CD, or CP) number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- GCRV Gen. Cat. of Radial Velocities (GCRV) number number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- PM_Name Name from other proper-motion catalog number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- HR Bright Star = Harvard Revised catalog <V.50> number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- Vys Number in red dwarf lists of Vyssotsky number= Star sequence numbers less than 1000 are from Gliese (1957); new stars have a number > 9000; The Sun is #0 (and therefore lacks entries in fields such as the RA and Dec. number= "S" indicates spectroscopic parallax number= J = combined components of binary V = variable velocity number= i.e GCdist represents parsecs if the Sun distance is 10kpc. See also in file "adc.doc" number= 1 = I or c; 2 = II or c; 3 = III or g; 4 = IV or sg; 5 = V or d; 6 = VI or sd; 7 = D or wd. Intermediate classes have no codes, e.g. 4 is given for IV-V. number= 1 if MK; 2 if combined MK type for multiple system; 4 if combined non-MK; blank if non-MK. number= J = combined light for multiple system P = Mag indicates a photographic magnitude V = variable magnitude number= Visual magnitude is reported to 0.01 mag if both probable error of parallax < 10% and V is given to 0.01 mag. --- Remark1 First remark code number=2 the codes are 2 = spectroscopic binary 3 = spectroscopic triple 4 = unresolved double, unknown nature 5 = UV Ceti flare star 6 = eclipsing binary 7 = semi-regular variable 8 = astrometric binary 9 = planetary nebula --- Remark2 Second remark code number=2 the codes are 2 = spectroscopic binary 3 = spectroscopic triple 4 = unresolved double, unknown nature 5 = UV Ceti flare star 6 = eclipsing binary 7 = semi-regular variable 8 = astrometric binary 9 = planetary nebula --- adc.doc Original Documentation by Wayne H. Warren Jr. Francois Ochsenbein CDS James Gass SSDOO/ADC 1997 Jul 21 UNKNOWN UNKNOWN * 19-Jul-1994: The file has been reformatted at CDS from the CD-ROM version "Selected Astronomical Catalogues Vol.1" with addition of decimal points when required (blank numbers in the decimal part) and conversion of RVel and Mag codes. * The 1950 declination of Gliese 157B (record #350) was corrected. * 21-Jul-1997: This document was brought up to current CDS/ADC standards. [J. Gass, ADC] V_32A.xml A Kinematic Abundance Survey at the Galactic Poles 5033 V/33 Kinematic Abundance Survey at Galactic Poles A Kinematic Abundance Survey at the Galactic Poles W I Hartkopf K M Yoss Astron. J. Vol. 87, No. 12, p. 1679 ??? ??? 1982 1982AJ.....87.1679H Photometry, DDO Radial velocities Photometry, narrow-band Galactic pole, north Galactic pole, south DDO observations of 1076 G and K stars at the north and south galactic poles have been combined with published photometry. Additional DDO photometry of bright field stars has been used to calibrate the DDO abundance index against [Fe/H] for metal-poor stars. Radial velocities were obtained for 302 of the polar giants, and coupled with published velocities.
Average Values for DDO, Mg Photometry cat Source of the identification 1. HD = Henry Draper 2. BD = Bonner Durchmusterung 3. UP = Upgren A.R. 1962 Astron. J. 67, 37. 4. MA = Malmquist K.G. 1936 Stockholm Ann. 12, #7. 1960 Uppsala Ann. 4, #9. 5. BOK = Bok B.J. and Basinski J. 1964 Mem. Mt. Stromlo Obs. 4, #1. 6. W = Weistrop D. 1981 Private Communication. 7. DL = Drilling J. and Lee P. 1979 Private Communication 8. PAJ = Jennens P.A. Mon. Not. R. Astron. Soc. 172, 695. --- name Identification Name --- RAh Right Ascension hours (1950) h RAm Right Ascension minutes min RAs Right Ascension seconds s DE- Declination sign --- DEd Declination degrees deg DEm Declination arcminutes arcmin DEs Declination arcseconds arcsec C48-45 48-45 Color --- C45-42 45-42 Color --- C41-42 41-42 Color --- C51-48 51-48 Color Magnesium Index (Clark J.P.A. and Mc Clure R.D (1979) Publ. Astron. Soc. Pac. 91, 507.) --- Reg Region Region and Category 1. NGP - Hartkopf W.I. and Yoss K.M. 1982 Astron. J. 87, #1523. 2. STD - Standards for Above Reference. 3. SGP - Yoss K.M. and Hartkopf W.I. 1979 Astron. J. 84, 1293. - Hartkopf W.I. and Yoss K.M. 1982 Astron. J. 87,#1523. 4. SA - Selected Areas - Yoss K.M., Karman R.A., and Hartkopf W.I. 1981 Astron. J. 86, 36. 5. IRS, IDS = Colors Derived from KPNO IRS and IIDS Spectra --- Cat Category --- Individual Observations for DDO, Mg Photometry cat Source of the identification See note for means.dat. --- name Identification Name --- RAh Right Ascension hours (1950) h RAm Right Ascension minutes min RAs Right Ascension seconds s DE- Declination sign --- DEd Declination degrees deg DEm Declination arcminutes arcmin DEs Declination arcseconds arcsec C48-45 48-45 Color --- C45-42 45-42 Color --- C41-42 41-42 Color --- C51-48 51-48 Color Magnesium Index (Clark, J.P.A. and Mc Clure, R.D. (1979) Publ. Astron. Soc. Pac. 91, 507.) --- Reg Region See note for means.dat. --- Cat Category --- Radial Velocities for NGP & SGP Stars cat Source of the identification See note for means.dat. --- name Identification Name --- RAh Right Ascension hours (1950) h RAm Right Ascension minutes min RAs Right Ascension seconds s DE- Declination sign --- DEd Declination degrees deg DEm Declination arcminutes arcmin DEs Declination arcseconds arcsec RV Radial Velocity Reduced to Sun km/s e_RV Mean Error of Velocity km/s o_RV Number of Observations --- code Telescope(s) Used Code for Telescope(s) Used - Hartkopf W.I. and Yoss K.M. (1982) -------------------------------------------------------------------------------- TABLE V. Accuracies of radial-velocity observations (in km/s). ------------------------------------------------------------------------ Telescope/ Dispersion Error measurements** Observer Year spectrograph (A/mm) Meas. Int. Obs. Ext. Code WIH 1978 KPNO 2.1-m/regular 78 2.6 1.8 5.7 6.5 K KMY 1978 CTIO 1.0-m/image tube 43 1.6 5.8 3.1 Y WIH 1979 CTIO 1.0-m/image tube 43 4.1 1.8 2.9 6.0 Y WIH 1980 CTIO 1.0-m/image tube 43 2.0 3.6 6.5 7.8 Y KMY 1978 CTIO 1.5-m/regular 39 1.7 2.4 9.2 13.0* C KMY 1979 KPNO coude feed/CIT 15 0.9 1.7 5.0 F WIH 1980 KPNO 2.1-m/IIDS 29 1.8 3.9 5.4 D WIH 1981 KPNO 2.1-m/IIDS 29 1.6 5.4 6.1 D WIH 1981 KPNO 0.9-m/IRS 46 2.1 9.5 4.8 I ------------------------------------------------------------------------ ** Error measurements are as follows: Meas.: rms error for repeated measurements of same spectrum. Int.: rms internal error from cross correlations. Obs.: rms error for multiple observations of one star. Ext.: rms external error (observed-published velocities). * Half weight for bright stars. --- Julie Anne Watko SSDOO/ADC 1996 Apr 17 V_33.xml A Supplement to the Bright Star Catalogue 5036B V/36B Supplement to the Bright Star Catalogue A Supplement to the Bright Star Catalogue E D Hoffleit M Saladyga P Wlasuk Yale University Obs. ??? ??? 1983 1983bscs.book.....H V/50 : Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991) Aitken, R. G. 1932, New General Catalogue of Double Stars within 120 degrees of the North Pole, Carnegie Institution of Washington Pub. 417 (Washington: Carnegie Institution of Washington). Cannon, A. J. and Pickering, E. C. 1918-1924, The Henry Draper Catalogue, Ann. Astron. Obs. Harvard College 91-99. (Cat. <III/135>) Couteau, P. 1978, Circ. Inf. No 75 (Meudon: IAU Commission des Etoiles Doubles). See also catalog <I/209> Hoffleit, D. (with the collaboration of Jaschek, C.) 1982, The BRIGHT STAR CATALOGUE, 4th revised edition (New Haven: Yale University Observatory ; see catalog <V/50>). Hoffleit, D., Saladyga, M. and Wlasuk, P. 1984, A Supplement to the Bright Star Catalogue (New Haven: Yale University Observatory). Jeffers, H. M., van den Bos, W. H. and Greeby, F. M. 1963, Index Catalogue of Visual Double Stars, Publ. Lick Obs. 21. Kholopov, P. N., Kukarkina, N. P. and Perova, N. B. 1978, 63rd Name-List of Variable Stars, Inf. Bull. Variable Stars, No. 1414. (See catalog <II/139>) Kholopov, P. N., Kukarkina, N. P. and Perova, N. B. 1979, 64th Name-List of Variable Stars, Inf. Bull. Variable Stars, No. 1581. (See catalog <II/139>) Kholopov, P. N., Samus', N. N., Kukarkina, N. P., Medvedeva, G. I. and Perova, N. B. 1981, 65th Name-List of Variable Stars, Inf. Bull. Variable Stars, No. 1921. (See catalog <II/139>) Kholopov, P. N., Samus', N. N., Kukarkina, N. P., Medvedeva, G. I. and Perova, N. B. 1981, 66th Name-List of Variable Stars, Inf. Bull. Variable Stars, No. 2042. (See catalog <II/139>) Kukarkin, B. V., Kholopov, P. N., Artiukhina, N. M., Fedorovich, V. P., Frolov, M. S., Goranskij, V. P., Gorynya, N. A., Karitskaya, E. A., Kireeva, N. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Ponamareva, G. A., Samus', N. N. and Shugarov, S. Yu. 1982, New Catalogue of Suspected Variable Stars (Moscow: Publishing Office <<Nauka>>). (See catalog <II/140>) Kukarkin, B. V., Kholopov, P. N., Efremov, Yu. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Pskovsky, Yu. P., Fedorovich, V. P. and Frolov, M. S. 1971, First Supplement to the Third Edition of the General Catalogue of Variable Stars (Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.). (See catalog <II/139>) Kukarkin, B. V., Kholopov, P. N., Efremov, Yu. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Pskovsky, Yu. P., Fedorovich, V. P. and Frolov, M. S. 1974, Second Supplement to the Third Edition of the General Catalogue of Variable Stars (Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.). (See catalog <II/139>) Kukarkin, B. V., Kholopov, P. N., Fedorovich, V. P., Kireyeva, N. N., Kukarkina, N. P., Medvedeva, G. I. and Perova, N. B. 1977, 62nd Name-List of Variable Stars, Inf. Bull. Variable Stars, No. 1248. (See catalog <II/139>) Kukarkin, B. V., Kholopov, P. N., Kukarkina, N. P. Kurochkin, N. E., Medvedeva, G. I., Perova. N. B., Pskovsky, Yu. P., Fedorovich, V. P. and Frolov, M. S. 1976, Third Supplement to the Third Edition of the General Catalogue of Variable Stars (Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.). (See catalog <II/139>) Kukarkin, B. V., Kholopov, P. N., Pskovsky, Yu. P., Efremov, Yu. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Fedorovich, V. P. and Frolov, M. S. 1969-70, General Catalogue of Variable Stars, 3rd edition (Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.) (See catalog <II/139>) Schmitz, M., Brown, L. W., Mead, J. M. and Nagy, T. A. 1978, Merged Infrared Catalogue, NASA TM-79683. (Catalog <II/71>) Smithsonian Astrophysical Observatory Staff 1966, Star Catalog. Positions and Proper Motions of 258,997 Stars for the Epoch and Equinox of 1950.0, Pub. of the Smithsonian Institution of Washington, D.C. No. 4652 (Washington: Carnegie Institution of Washington; see catalog <I/131>) Worley, C. E. 1982, in IAU Colloquium No. 64, Automated Data Retrieval in Astronomy, Ed. C. Jaschek and W. Heintz (Dordrecht: D. Reidel Publishing Company), p. 257. (see catalog <I/237>) Combined data Stars, bright The catalog is an extension of the BSC4 (Hoffleit 1982; see catalog <V/50>) and contains compiled data on stars for which photoelectric determinations are given as 7.10V or brighter and that are not already included in the latter catalog. The data included in the supplement are basically the same as those in the BSC4 itself, and the format of the machine version is very similar. Notable differences are that the NAME column has been omitted, since very few supplement stars have Bayer or Flamsteed designations, and has been replaced with the SAO number. Also, the parallax field includes only data determined from trigonometric methods; all dynamical parallax data have been relegated to the REMARKS. Position-angle data are given in the main table for double stars, whereas they were contained, if reported, only in the REMARKS file of the BSC4. Remarks for supplement stars are given in a separate file of the machine version and are present for 49% of the stars. The introductory file "intro.doc" contains the text given in the introduction to the published catalog except that the figures are, of course, not included. Data included in the catalog "bsc4s.dat" are HD number; DM number; SAO number; double-star code or identification; variable-star identification; right ascension (B1900) declination, right ascension (B2000) declination; galactic coordinates; V magnitude; B-V, U-B, R-I colors; spectral type; annual proper motions; parallax; radial velocity (km/s): and projected rotational velocity v sin i (km/s). Data included for multiple stars are magnitude difference, separation (arcsec), position angle (PA) of components, component identifications (A, B, ...), and number of components (N). A remarks flag is included as a pointer to a remarks file. The third file "remarks.dat" contains the actual remarks for stars flagged in the data file.
The Supplement to the Bright Star Catalogue HD Number in the Henry Draper Catalogue <III/135> --- m_HD HD suffix. May be component identifications used for multiple systems, or /X when more than a single HD star is included, e.g. HD 17245/6. NOTE: m_HD is "S" for the 3 stars not in HD catalogue, for which the SAO number is listed in column HD; those stars are SAO 250043 (CP-60 980), SAO 179278 (BD-20 3283) and SAO 252421 (CP-61 3926) --- DM Durchmusterung (BD, CD, CPD) designation --- SAO Catalog number in SAO <I/131> --- Iflag "I" if the star occurs in the NASA Merged Infrared Catalogue <II/71> --- ADS Double or multiple star identifications spectroscopic and eclipsing binaries are not considered here. The field is uniform with the catalog codes in byte 28, ADS numbers in bytes 29-33, and multiple-star letter designations for components of a system which the HD number represents in bytes 34-35. Other designations include: W Worley (1978; see Worley 1982) update of the IDS (Jeffers et al. 1963) (see catalog <I/237>) C Couteau 1978 (see catalog <I/209>) D Duplicity discovered by occultation --- Vname Variable-star designations these designations include: (a) constellation designations from the General Catalogue of Variable Stars (see 4th Edition as Catalog <II/139>) (b) numbers (alone) from the New Catalogue of Suspected Variable (see latest version in Catalog <II/140>) (c) Var and Var? for unnamed variables and suspected unconfirmed variables not included in the General and Suspected catalogs. Can apply to the HD number and/or a close companion. Note: HD 139216 = Tau4 Ser is recorded as "@t|4 Ser" where the character following the t is a vertical bar. --- RAh Right Ascension 1900 (hours) h RAm Right Ascension 1900 (minutes) min RAs Right Ascension 1900 (seconds) s DE- Declination 1900 (sign) --- DEd Declination 1900 (degrees) deg DEm Declination 1900 (minutes) arcmin DEs Declination 1900 (seconds) arcsec RAh2000 Right Ascension 2000 (hours) h RAm2000 Right Ascension 2000 (minutes) min RAs2000 Right Ascension 2000 (seconds) s DE-2000 Declination 2000 (sign) --- DEd2000 Declination 2000 (degrees) deg DEm2000 Declination 2000 (minutes) arcmin DEs2000 Declination 2000 (seconds) arcsec GLON Galactic longitude. deg GLAT Galactic latitude. Sign always in deg Vmag V magnitude on UBV system. Magnitudes of variables and/or binaries may be reported to 0.1 mag only. mag u_Vmag Uncertainty flag (:) on Vmag --- B-V B-V colour index mag U-B U-B colour index mag R-I colour on system indicated by n_R-I mag n_R-I Code for R-I system this code may be a colon indicating a larger uncertainty, or (blank) - on Johnson system; E - mainly from Eggen, on Kron system; C - from Cousins, close to Kron system (the Johnson and Kron filters have different passbands and may not be used interchangeably). --- SpType Spectral type. If the complete modern (MK) classification is too long for the data field, it is given in the remarks file and an asterisk (*) occurs in this data field. Mt. Wilson luminosity classes are given as lower case letters in bytes 128-129. The "W" in Wolf-Rayet types is in byte 129 with the C or N in the following byte (130). In general, the temperature class (O, B, A, ..., S, C) occurs in byte 130 and the temperature subclass in byte 131 (intermediate sub-classes extend to 132-133 and other characters can be in bytes 131, ...). Characters normally appearing as lower case in standard notation, e.g. p, e, Si, Mn, Hg, Iab, are coded in lower case. A greek delta appearing for HD 189337 is coded as "@d". --- pmRA Annual proper motion in right ascension. arcsec/yr pmDE Annual proper motion in declination. arcsec/yr Plx Trigonometric parallax. Dynamical parallaxes are given in the remarks file. arcsec RVel Radial velocity (see codes in n_RVel) field). km/s n_RVel Radial-velocity code the peculiarities are: V, V? - variable or suspected variable velocity; SB, SB1, SB2 - spectroscopic binaries, single or double lined spectra; O - orbital data available. One star (HD 2268) has a velocity with one decimal (0.5) stored there. --- l_vsini Limit indicators for vsini --- vsini Projected rotational velocity v.sin i. km/s u_vsini Colon (:) for uncertain v sin i (no occurrences at present). --- Dmag Differential magnitude difference magnitude difference between two components of a double, or between the two brightest components of a multiple system. mag u_Dmag Differential magnitude code. this code takes the values V indicates variable magnitude difference, : uncertainty indicator (:); no occurrences at present. --- Sep Separation of the components "Comp" arcsec n_Sep Separation code "a" occurs if the separation refers to the semimajor axis . The colon (:) indicates, as usual, a large uncertainty. --- PAcomp Position angle for the components "Comp" this field may contain "ORB" to indicate an available orbit; hence, no PA. "SP" to indicate south preceding, "SF" to indicate south following, and "S" to indicate south. deg u_PAcomp PA code (: for uncertainty). --- Comp Identification of components. Identification of components represented in bytes 185-188 and 191-195. The character "O" indicates an occultation binary. --- Ncomp Number of components assigned to multiple systems. --- Remark An asterisk indicates that further information can be found in the remarks file. --- *Remarks to stars in the catalogue HD HD (SAO in 3 cases) number, as in file bcs4s.dat --- m_HD HD suffix (or "S" for SAO), as in file bcs4s.dat --- Category Remark category abbreviation the categories are: C: magnitudes, colors, color excesses; D: double and multiple stars, including astrometric and those discovered by occultations and speckle interferometry. Orbital data given, including magnitudes and spectral types of major components, orbital periods, semimajor axes, etc.; Dyn: dynamical parallaxes; G: membership in clusters, associations, groups and apparent association N: star names and identifications; R: stellar radii or diameters; with nebulosity (R associations). No attempt made to resolve conflicting assignments in different sources: various alternatives are included; RV: radial and rotational velocities; S: spectra; SB: spectroscopic binaries, mostly orbital data: period of revolution, K = half amplitude of radial velocity, K$1, k$2 = semi-amplitude in RV for each of the components of SB2 system, V$0 = mean radial velocity of the system, msin3i = mass function in Solar masses, asini = projected semimajor axis in Gm (10^6^km) ; Var: variability, magnitude ranges, spectrum or magnetic field variability or other characteristics; M: miscellaneous notes. --- --- Left parenthesis --- Cont Continuation letter --- --- Right parenthesis --- Text Remarks in free text form. --- intro.doc Introduction to the catalogue Francois Ochsenbein CDS 1997 Apr 08 Appreciation is expressed to Dr. E. Dorrit Hoffleit and her colleagues for preparing and sending the magnetic tape of the catalog. Dr. Hoffleit kindly communicated additional corrections to the catalog and reviewed this document in preprint form before final printing. A large part of this ReadMe file was generated from the "Documentation for the machine-readable version of 'A Supplement to the Bright Star Catalogue'" by Wayne H. Warren Jr. made in February 1984 (document NSSDC/WDC-A-R&S 84-04) V_36B.xml The Fourth Catalog of Orbits of Visual Binary Stars 5039 V/39 4th Catalog of Orbits of Visual Binaries The Fourth Catalog of Orbits of Visual Binary Stars C E Worley W D Heintz Publ. U.S. Naval Obs. 2 24, ??? ??? 1983 1983PUSNO..24g...1W Binaries, orbits Stars, double and multiple The Finsen-Worley Catalog (1970), supplemented by all subsequently published orbits known to Worley and Heintz as of 1 July 1982 formed the basis for the present compilation. Practically all stars having visual orbits were reobserved in the preceding decade, often repeatedly either with micrometers or with speckle interferometers. Astrometric solutions are included but only if they were judged to be relatively certain. Orbits with period greater than 4000 years and hyperbolic orbits were rejected as being unreliable. The catalog contains 928 orbits of 847 systems (counting triples as two systems). There are 23 orbits of unresolved systems. The catalog contains for each system the names of the star and the components involved, the 1900 position, the ADS number, the magnitude and spectral type for each component, the orbital elements, the equinox of the node, the quality of the orbit, the date of the last observation, the inclusive dates for which an ephemeris is given by the author, the computer of the orbit, and a reference.
4th Catalogue of Orbits of Visual Binary Stars RAh Hours RA, 1900.0 h RAm Minutes RA, 1900.0 min DE- Sign Dec, 1900.0 --- DEd Degrees Dec, 1900.0 deg DEm Minutes Dec, 1900.0 arcmin Note '*' indicates a note in file "notes" --- ADS Aitken's Double Star Catalog (ADS) designation --- MagA Magnitude of component A mag n_MagA 'V' if MagA is variable --- MagB Magnitude of component B mag n_MagB 'V' if MagB is variable --- Period Period of the binary star orbit a Axis Semi-major axis of the orbit arcsec Incl Inclination (i) of the orbit deg Omega Position of the Node deg n_Omega '*' if Omega is identified as the ascending node --- n_Grade 'A' indicates ambiguities (see intro) --- Grade The grade from 1 (definitive) to 5 (indeterminate), see file intro --- DateObs Date of last observation used in computation a Author Computer of the orbit --- Name Common names of the star --- SpTypeA Spectral type of component A --- SpTypeB Spectral type of component B number=1 An '*' following this value indicates the spectral types have been inferred from a combined spectrum and a known magnitude difference. --- PeriT Time of periastron passage a Ecc Eccentricity --- omega Longitude of Peri reckoned from Omega deg Eqomega Equinox of Omega a Ephem Inclusive dates of ephemeris --- Ref Text of bibliographic reference --- Notes about flagged orbits RADec Name based on 1900 position, form "HHMMm+DDMM" --- Note Notes --- intro.doc Introduction to the Catalogue Francois Ochsenbein CDS Catalogues Service 1995 Mar 02 UNKNOWN UNKNOWN * From the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory /combined/binorbit * 02-Mar-1995: hours of RA (29) in record # 793 corrected * 23-Sep-1996: aligned record #642 (Gail L. Schneider) * 16-Oct-1996: corrected the "Note" flag (catalog) and RADec values (notes) to ensure the correspondance. V_39.xml Catalog of Orbital elements, Masses and Luminosities of close double stars 5042 V/42 Close double stars Catalog of Orbital elements, Masses and Luminosities of close double stars M A Svechnikov L A Bessonova Bull. Inform. CDS 26 99 1984 1984BICDS..26...99S Binaries, orbits This catalogue is a new edition of the catalogue of the photometric and absolute elements of close double systems by Svechnikov (ref 142). After the appearance of this catalogue(1969), the numerous new data concerning both photometric and spectroscopic elements of orbits of the eclipsing binaries were published. The precision of determination of the light curves of eclipsing systems is essentially augmented; now, the light curves of eclipsing binaries are obtained mainly by means of multicolour photoelectric observations; for a number of systems,e extra-atmospheric observations from satellites and orbital astronomical observatories are available. More details are available in original.doc.
Summary of close binaries Name Designation of the Eclipsing Binary --- HD Designation in Henry Draper Catalogue --- Type Eclipsing binary type --- Group of classification (see intro.ori) --- Seq Number of the system used in table2 and table3 --- Note e.g. other possible class (see intro.ori) --- Photometric elements Seq Number of the system --- Name Designation of the System --- Period Period d n_Period '*' indicates a variability of Period --- Type of eclipse (see intro.ori) --- R1 Mean fractional radius number=2 The mean fractional radius (or the small equatorial semi-axes of ellipsoidal stars which are, within the limits of errors of evaluation of photometric elements, practically equal to the mean radii) relative to the orbital major semi-axis --- n_R1 Notes on R1 number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) --- R2 Mean fractional radius number=2 The mean fractional radius (or the small equatorial semi-axes of ellipsoidal stars which are, within the limits of errors of evaluation of photometric elements, practically equal to the mean radii) relative to the orbital major semi-axis --- n_R2 Notes on R2 number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) --- b/a Ratio of minor to major axis --- n_b/a Notes on B/A number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) --- i Orbital inclination angle deg n_i Notes on i number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) --- LimbCoef Used limb-darkening coefficient number=3 if the values of the limb-darkening coefficient of the components are not equal, these are given in the notes (file notes) --- n_LimbCoef Notes on LimbCoef number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) --- L1 Fractional light (relative to L1+L2) --- n_L1 Notes on L1 number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) --- L2 Fractional light (relative to L1+L2) --- n_L2 Notes on L2 number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) --- J1/J2 ]0/]? Ratio of surface brightness number=4 ratio of surface brightness found from the photometric solution; if the geometric elements of the system obtained from several different (but very similar) photometric solutions are averaged, J1/J2 are calculated with the averaged values of the radii of the components. --- n_J1/J2 Notes on J1/J2 number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) --- Passband Wavelength domain 0.1nm l_Weight Limit flag (<) on Weight --- Weight on the reliability of photometric elements (See Svechnikov, ref 142) --- Com Comments number=5 Figures '1' and '2' designate the cases, when 2 essentially different variants of the photometric solutions for the same eclipsing system exist, and when we are not able to prefer one of these cases (as a rule, however, only those photometric solutions are given) which seem to be (in opinion of the authors of this catalogue) the most realistic. The data concerning the other photometric solutions (or corresponding bibliographic references) are mentioned in the notes. --- Absolute elements Seq Number of the system --- Sp Spectral classes --- q Mass ratio M2/M1 number=2 Mass-ratios found spectroscopically, from double-lined spectroscopic orbit, are not accompanied by additional marks. The values of q estimated by means of the so-called 'M-L method', using the mass-function obtained from single-lined spectral orbit, and assuming,that primary component satisfies the mass-luminosity relation for the main-sequence-stars (see Kopal, ref 371;823; Svechnikov, ref 142), are enclosed in brackets. The values of q estimated by some other method, as well as averaged values of q, are accompanied by the asterisks. --- n_q Note on q number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; the bracket ')' very questionable values (the original left bracket has been removed) exclamation '!' is not explained in the "intro.ori" file --- M1 Mass of first component solMass q_M1 Uncertainty flag (:) on M1 --- M2 Mass of second component solMass q_M2 Uncertainty flag (:) on M2 --- a Orbital semi-major axis solRad Rad1 Radius of first star solRad n_Rad1 Note on Rad1 number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; the bracket ')' very questionable values (the original left bracket has been removed) exclamation '!' is not explained in the "intro.ori" file --- Rad2 Radius of second component solRad q_Rad2 Uncertainty flag (:) on Rad2 --- Mbol1 Absolute Bolometric magnitude of component 1 number=3 The absolute bolometric magnitudes are computed using the geometric and spectroscopic characteristics of the components yielded in the previous columns; the stellar effective temperatures given in Popper's (ref 1615) survey (and based mainly on the scale of effective temperatures and bolometric corrections of Hayes, ref 1623) are used. mag n_Mbol1 Note on Mbol1 number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; the bracket ')' very questionable values (the original left bracket has been removed) exclamation '!' is not explained in the "intro.ori" file --- Mbol2 Absolute Bolometric magnitude of component 2 number=3 The absolute bolometric magnitudes are computed using the geometric and spectroscopic characteristics of the components yielded in the previous columns; the stellar effective temperatures given in Popper's (ref 1615) survey (and based mainly on the scale of effective temperatures and bolometric corrections of Hayes, ref 1623) are used. mag n_Mbol2 Note on Mbol2 number=1 The '*' indicates a note (see file notes) the colon ':' a questionable value; the bracket ')' very questionable values (the original left bracket has been removed) exclamation '!' is not explained in the "intro.ori" file --- l_W2 Lower limit (<) on W2 --- W2 Weight on the accuracy of determination of the absolute elements. number=4 see Svechnikov, ref 142 --- Comment Comments number=5 Figures '1' and '2' indicate the cases, when 2 different variants of the absolute elements are obtained (corresponding to 'case 1' and 'case 2' of the evaluation of photometric elements or to 2 considerably different estimates of q). Also,in this column, the number of the group for US-systems is indicated as well as some other important remarks. --- original.doc Original introduction Nancy G. Roman ADC 1995 Feb 02 This document was prepared by Francois Ochsenbein of the CDS in October, 1994. It was modified by the inclusion of the ADC keywords and of a more extensive description. V_42.xml Catalogue of Masses and Ages of Stars in Twelve Open Clusters 5043 V/43 Masses and Ages of Stars in Twelve Open Clusters Catalogue of Masses and Ages of Stars in Twelve Open Clusters V I Myakutin R Sagar U C Joshi CDS Bull. No. 26, p. 103 ??? ??? 1984 1984BICDS..26..103M Clusters, open Stars, masses Stars, ages In this catalogue the evolutionary masses and ages of about 1030 stars in 12 open clusters for which the UBV photoelectric photometry has been carried out at the U.P. State Observatory, Nainital, India are listed. The mass and age of a star can be estimated by its position in the H-R diagram using the theoretical evolutionary tracks of stars with different masses. In comparison to field stars, members of an open cluster are more suitable objects for such calculations because of the homogeneous chemical composition in the clusters and the reliability of luminosities and temperatures determined from the cluster UBV data (Piskunov, 1980) See the list of clusters in the Note(1) below.
The catalogue Cl Cluster designation number=1 The list includes the following clusters: -------------------------------------------------- NGC Cluster# Rup m-M E(B-V) Ref -------------------------------------------------- A = 581 C0129+604 326 12.05 0.38 [1] B = (TR1) C0132+610 328 11.64 0.52 [2] C = 654 C0140+616 330 10.85 [3] D = (IC1805) C0228+612 352 11.90 [4] E = 1778 C0504+369 429 11.09 0.34 [5] F = 2169 C0605+139 481 10.04 0.18 [6] G = 2264 C0638+099 495 9.50 [7] H = 2539 C0808-126 611 10.60 0.11 [8] I = 6530 C1801-243 19 11.20 [9] J = 6611 C1816-138 54 12.50 [10] K = 6823 C1941+231 124 12.70 [11] L = 6913 C2022+383 168 10.40 [12] -------------------------------------------------- --- Seq Sequential number of the star --- Ident Designation of the star number in the UBV source --- V V magnitude mag B-V color index mag U-B color index mag E(B-V) Color excess mag Memb Membership indicator --- LC Lumminosity Class --- logTe Effective temperature K logL Luminosity Sun Age Star age yr Mass Mass of the star Sun Pr Probability of estimated mass and age --- Francois Ochsenbein CDS James Gass SSDOO/ADC 1997 Jul 29 V_43.xml A Catalogue of Classical (Evolved) Algol-Type Binary Candidate Stars 5046 V/46 Classical A Catalogue of Classical (Evolved) Algol-Type Binary Candidate Stars E Budding CDS Bull. No. 27, p. 91 ??? ??? 1984 1984BICDS..27...91B II/139 : General Catalog of Variable Stars (GCVS), 4th Ed. (Kholopov+ 1988) II/150 : Parameters for eclipsing binaries (Brancewicz+, 1980) Awadalla, N.S. and Budding, E.: 1980. The Observatory, 100, 108. =1980Obs...100..108A Bachmann, P.S. and Hershey, J.L.: 1975, Astr. J. 80., 836. =1975AJ.....80..836B Barnes, R.C.: 1974, Pub. Astr. Soc. Pacific, 86, 195. =1974PASP...86..195B Batten, A.H.: 1973, Binary and Multiple Systems of Stars, Pergamon Press. Brancewicz, H.K. and Dworak, T.Z.: 1980, Acta Astr. 30, 501. =1980AcA....30..501B, catalog <II/150> Budding, E.: 1981, in "Investigating the Universe" (ed. F.D.Kahn). Reidal,p.271. Budding, E.: 1982, Proceedings IAU Colloquium No.69, Binary and Multiple Stars as Tracers of Stellar Evolution, ed. Z.Kopal and J.Rahe, Reidel,p.351. Budding, E.: 1983, Proceedings of IAU Colloquim No.80, Double Stars: Physical Properties and Generic Relations, ed. Z. Kopal and J. Rahe, Astrophys. Sp. Sci., 99, 299. =1984Ap&SS..99..299B Budding, E. and Najim, N.N.: 1980, Astrophys. Sp. Sci., 72, 369. =1980Ap&SS..72..369B Carpenter, E.F.: 1930, Astrophys. J. 72, 205. Cester, B., Fedel, B., Giuricin, G., Mardirossian, F. and Pucillo, M.: 1977, Astr. Astrophys., 61, 469. =1977A&A....61..469C Cester, B., Fedel, B., Giuricin, G., Mardirossian, F. and Mezzetti, M.: 1978b Astr. Asrophys. Suppl., 33, 91. =1978A&AS...33...91C Cester, B., Giuricin, G., Mardirossian, F., Mezzetti, M., Maceroni, C. and Mancuso, S.: 1979a, Astr. Astrophys., 73, 31. =1979A&A....73...31C Cester, B., Giuricin, G., Mardirossian, F., Mezzetti, M. and Milano, L.: 1979b, Astr. Astrophys. Suppl., 36,273. =1979A&AS...36..273C Gaposchkin, S.: 1940, Harvard Reprint, No. 201. Giannone, P. and Giannuzzi, M.A.: 1974, Astrophys. Sp. Sci., 26, 289. Giuricin, G. and Mardirossian, F.: 1981a, Astrophys. J. Suppl. 46, 1. =1981ApJS...46....1G Giuricin, G. and Mardirossian, F.: 1981b, Astr. Astrophys. Suppl. 45,85. =1981ApJS...46....1G Giuricin, G. Mardirossian, F. and Mezzetti, M.: 1983, Astrophys. J. Suppl. 52,35. =1983ApJS...52...35G Hall, D.S.: 1974, Acta Astr., 24, 215. Hall, D.S.: 1976, Proceedings of IAU Colloquim No.29, Multiple Periodic Variable Stars, ed. W. Fitch, p. 287. Hall, D.S. and Cannon, R.O.: 1974, Acta Astr.,24, 79. Hall, D.S. and Neff, S.G.: 1979, Acta Astr.,29, 641. =1979AcA....29..641H Jakate, S., Bakos, G.A., Fernie, J.D. and Heard, J.F.: 1976, Astr. J. 81, 250. =1976AJ.....81..250J Kandpal, C.D.: 1975, Astrophys. Sp. Sci. 32, 291. Koch, R.H., Plavec, M. and Wood, F.B.: 1970, Publ. Univ. Penn. Astr. Series, Volume XI, pl. Kondo, Y., Mcluskey, G.E. and Parsons, S.B.: 1983, Proceedings of Colloquium No. 80, Double Stars: Physical Properties and Generic Relations, ed. Z. Kopal and J. Rahe (to be published as a Volume of Atsrophys. and Sp. Sci.), Reidel, (in press). Kopal, Z.: 1955,Ana. d'Astrophys. 18, 379. =1955AnAp...18..379K Kopal, Z.: 1959, Close Binary Systems, Chapman and Hall, London. Kukarkin, B.V., Kholopov, P.N., Efremov, Y.N., Kukarkina, N.P., Kurochkin, N.E., Medvedeva, G.I., Perova, N.B., Fedorovich, V.P. and Frolov, M.S.: 1969, General Catalogue of Variable Stars (Vol I - 3rd edition), also Vol II (1970), and first (1971) and second (1974) supplements. Moscow. Labeyrie, A., Bonneau, D., Stachnik, R.V. and Gezari, D.Y.: 1974 Astrophys. J. (Letters) 194, L147. =1974ApJ...194L.147L Lacy, C.H.: 1979, Astrophys. J., 228, 817. =1979ApJ...228..817L Lubow, S.H. and Shu, F.H.: 1975, Astrophys. J. 198, 383. =1975ApJ...198..383L MacDonald, D.D.: 1964, McCormick Publ. 13, part 5, 51. Mardirossian, F., Mezzetti, M., Predolin, F. and Giuricin, G.: 1980, Astr. Astrophys. Suppl. 40, 57. =1980A&AS...40...57M Mancuso, S., Milano, L., Vittone, A., Budding, E. and Jassur, D.M.Z.: 1981, in Photometric and Spectroscopic Binary Systems, eds. E.B. Carling and Z. Kopal, Reidel, p.313. Morgan, J.G. and Eggleton, P.P.: 1979, Mon.Not. R. Astr. Soc. 187, 661. =1979MNRAS.187..661M Morton, D.C.: 1960, Astrophys. J. 132, 146. =1960ApJ...132..146M Packet, W.: 1980, Proceedings of IAU Symposium No.88, Close Binary Stars: Observations and Interpretation, ed. M.J. Plavec, D.M. Popper, R.K. Ulrich, Reidel, p.211. Paczynski, B.: 1971, Ann. Review Astr. Astrophys., 9, 183. =1971ARA&A...9..183P Plavec, M.: 1973, Proceedings of IAU Symposium No.51, Extended Atmospheres and Circumstellar Matter in Spectroscopic Binary Systems, ed. A.H. Batten, Reidel,p. 216. Plavec, M.: 1980, Proceedings of IAU Symposium No.88, Close Binary Stars: Observations and Interpretation, ed. M.J. Plavec, D.M. Popper, R.K. Ulrich, Reidel, p.251. Plavec, M.: 1984, UCLA Preprint No. 160. Plavec, M. and Polidan, R.S.: 1976, Structure and Evolution of Close Binary Systems, ed. P. Eggleton, Reidal, p.289. Popper, D.M.:Proceedings IAU Symposium No.6, Mass Loss and Evolution in Close Binaries, ed. K.Gyldenkerne and R.M.West, Copenhagen University Publications. Popper, D.M.: 1976, Astrophys. J., 206, 142. =1976ApJ...208..142P Popper, D.M.: 1978, Bull. A.A.S. 10, 608. Popper, D.M.: 1980, Ann. Rev. Astr. Astrophys. 18, 115. =1980ARA&A..18..115P Popper, D.M. and Ulrich, R.K.: 1977, Astrophys. J. (Letters) 212, L131. =1977ApJ...212L.131P Refsdal, S. and Weigert, A.: 1969, Astr. Astrophys. 1, 167. =1969A&A.....1..167R Rudy, R.J. and Kemp, J.C.: 1978, Astrophys. J., 221, 200. =1978ApJ...221..200R Sahade, J. and Wood, F.B.: 1978, Interacting Binary Stars, Pergmon Press. Schneider, D.P., Darland, J.J. and Leung, K.C.: 1979, Astr. J. 84, 236. =1979AJ.....84..236S Shapiro, L.T.: 1973, Ph.D.Thesis, Northwestern University, Illinois. An Investigation of 1400 Above-the-Main Sequence Close Binaries. Soderhjelm, S.: 1980, Astr. Astrophys., 89, 100. =1980A&A....89..100S Stothers, R.: 1973, Publ. Astr. Soc. Pacific, 85, 363. =1973PASP...85..363S Struve, O.: 1948, Ann. Astrophys. 11, 117. Struve, O.: 1949, Mon. Not. R. Astr. Soc. 109,487. Svechnikov, M.A.: 1969, Katalog orbitalnyich elementov, mass i svetimostei tesnyich dvoinyich zvezd, A.M.Gorky University of the Urals, Sverdlovsk. Szafraniec, R.: 1960, Acta. Astr., 10, 99. =1960AcA....10...99S Szafraniec, R.: 1970, Acta. Astr., 20, 26. =1970AcA....20...26S Szafraniec, R.: 1971, Acta. Astr., 21, 55. =1971AcA....21...55S Szafraniec, R.: 1972, Acta. Astr., 22, 273. =1972AcA....22..273S Szafraniec, R.: 1974, Acta. Astr., 24, 89. =1974AcA....24...89S Szafraniec, R.: 1976, Acta. Astr., 26, 25. =1976AcA....26...25S Tchudovichev, V.P.: 1952, Bull. Astr. Obs. Engelhardt, Kazan. No.28,1. Tomkin, J. and Lambert, D.L.: 1978, Astrophys. J. (Letters), 222, L119. =1978ApJ...222L.119T Walter, K.: 1931, Konigsberg Veroff., No.2. Walter, K.: 1979, Astr. Astrophys. Suppl. 37, 493. =1979A&AS...37..493W Wilson, R.E. and Rafert, J.B.: 1980, Astr. Astrophys. Suppl. 42, 195. =1980A&AS...42..195W Wood, D.B.: 1972, A Computer Program for Modelling Non-Spherical Eclipsing Binary Systems, Godard Space Flight Centre, Greenbelt, Maryland, U.S.A. (Also refer to WINK status reports, issued privately by D.B.Wood over the period 1973-1978.) Wood, F.B.: 1950, Astrophys. J. 112, 196. =1950ApJ...112..196W Wood, F.B., Oliver, J.P., Florkowski, D.R. and Koch, R.H.: 1980, Publ. Univ. Penn. Astr. Series v.12, Philadelphia. Binaries, eclipsing A catalogue of some 414 classical Algol-type binary candidates is presented. Apart from the entries on numerous well-known and studied Algols, the catalogue draws attention to a large number of probably similar but generally less well-known stars, as well as others which may have been cited as possible Algols, though for which the overall evidence appears weaker. Acronyms used: BD = Brancewicz and Dworak (1980) (catalog <II/150>) GM = Giuricin and Mardirossian (1981a) GCVS = General Catalog of Variable Stars <II/139>
The Catalogue ID Serial number of entry. --- Cont indicates a continuation of NEXT star --- name Name of star Arranged in alphabetical order of constellation listing (as in the General Catalogue (GCVS) of Kukarkin et al., 1969, 1970, 1971,1974) --- Per Period d mass Mass of the primary star The mass as given in the catalogue of Brancewicz and Dworak (1980) (hereafter BD), to two decimals. Sometimes an additional entry (above the BD mass) refers to some other recent estimates. This will usually be for the more well known Algol systems, the mass being that quoted by Giuricin and Mardirossian (1981a) (hereafter GM). solMass u_mass Uncertainty remark on mass --- Sp Spectral Type The MK spectral type(s) (when available) are almost always those of BD. A colon indicates uncertainty, while brackets refer to types which have been indirectly inferred by certain other light curve analysts (see BD for details).A few of the candidate stars are not listed by BD, in which case the types are probably those quoted by Kukarkin et al., (GCVS - op. cit.) or Wood et al.,(1980). --- q Mass ratio quoted by BD For many systems this comes from an initial trial value which is subsequently iteratively improved on, in order to make the system parameters (especially those of the primary star) fit in the prescribed correlations (see section 2 of the publication) to within some permitted tolerance. --- subVol Subgiant volume / Roche volume subVol (r(L2)) indicates BD's assessment of the volumetric percentage proportion of its limiting (Roche) lobe occupied by the subgiant component. In a majority of cases of candidate EA2 systems BD find this quantity to be less than 100 (i.e. an "undersize" implication). This could, however, reflect systematic errors of some adopted constant values in some of the formulae put together in order to effect solutions (Budding, 1983). In any case, the proximity of r(L2) to 100 is a good clue to the likelihood of an SD (semi-detached) system designation. % u_subVol Uncertainty remark on subVol --- l_qsd Limit or approximate flag on qsd --- qsd Calculated mass ratio The quantity q(SD) would usually denote the mass ratio calculated using BD's relative radius of the secondary component (R(2)/Sep), a quantity already determined in the light curve analysis as r(2), and Kopal's (1959) Table (3-2), which relates the mean relative radius of the component in an sd system, i.e. one which is in contact with its surrounding (inner) Roche critical surface (passing through the inner Lagrangian point), to the corresponding mass ratio. Again, as with the entries in mass, additional recently published values are sometimes also included above the main entry for more well known systems. Other possible entries for q(SD) will be referred to in the next section. --- n_qsd Remark on qsd --- l_Depth1 Limit flag on Depth1 --- Depth1 The importance of depth of primary minimum For certain eclipsing binary systems, that this is a salient observational parameter, by means of which likely sd candidates may be identified, was already stressed in Shapiro's (1973) thesis. This quantity was utilized by Budding (1981) to select light curves of EA2 type. It will indeed become clear on inspection of the candidate list that most of the more well known classical Algol systems have light curves of this type. The value of the depth is given in magnitudes. mag n_Depth1 Passband (as in GCVS). --- r1 Relative radius of primary The tenth column gives the relative radius of the primary component r(1), which is simply derived from (R(1)/Sep) as listed by BD. Like the previously mentioned r(2), this is a quantity which would normally be calculated from analysis of the photometric data, and though published results of such analyses often quote its value to three or more significant decimal digits, a two digit value is already an optimistic assessment of the likely information content for the majority of less well-known candidate stars. The extent of disagreement between different sources on such parameters for even the more well-known examples suggests that a two figure number is a realistic datum to insert here. This quantity can, of course, be combined with the mass, mass ratio and the period to allow absolute sizes of the system components to be derived. --- sd sd status The sd status could be regarded as a crude probability assessment of the semi-detached nature of the system. It takes the five values from 0.1 up to 0.9 in steps of 0.2. 0.9 will normally be placed alongside the well-known cases (such as most of those in the GM list), for which comparison information columns (4) and (8) is presented. A value 0.7 is associated with binaries of apparently similar superficial properties to the 0.9 cases, but such binaries appear to be relatively neglected. 0.5 goes with the binaries for which an EA2 or EA1 designation might be about equally likely, whereas the balance of probability would seem to be against a normal sd classification for the 0.3 systems. Those binaries with sd status 0.1 are regarded as definitely unlikely to represent classical evolved Algol systems. --- Remarks ID Serial number of entry. --- name Name of star The name is blank for continuation lines --- ref Reference to most recent well-known catalog K Koch et al., (1970) S Svechnikov, (1969) T Tchudovichev, (1952) G Gaposchkin, (1940) --- l_Q Less than sign --- Q Quality description The above sources usually refer to the quality of the original photometric data, or give some (numerical) indication as to their feelings of the overall reliability of their solutions. This has been put together here under the general quality descriptor Q, which may be interpreted in a similar way to the sd status measure, except that (since Svechnikov's `weights' are in a scale of 1-10) the values 0.2, 0.4 etc. might also appear. --- rem Remarks The remarks column offers a few words of additional information. In order to appreciate these, however, it will be necessary to understand the following abbreviations: BD The catalogue of Brancewicz and Dworak (see(4) above). C Cester et al. (1978b). EA Algol type light curve as defined by Kukarkin et al., (1969). EA1, Subdivisions of the EA type designation introduced EA2 by Budding (1981). EA1 refers to a pair of eclipsing unevolved Main Sequence dwarfs, giving rise to a light curve sometimes described as being of `Algol type'; though often with distinctive differences from that of an EA2 type system, which refers to evolved Algols forming the main subject of this article. G Gaposchkin's(1940) catalogue (see(12) and(13) above). GM Giuricin and Mardirossian (1981) (see(4) above). HN Hall and Neff (1979). k Ratio of relative radii (usually r(2)/r(1)). lc Light curve. mf Mass function. min Photometric minimum (Min II refers to the depth of the secondary minimum.). oc Occultation, i.e. eclipse formed by the larger star obscuring the smaller one. q Ratio of masses (i.e. M lesser/M greater = M(2)/M(1)). RS A system containing an "undersize" subgiant. Special attention was called to these systems by Kopal (1959) and also (using the same designation, though with a slightly more restricted meaning, by Svechnikov (1969). Many systems of this type have since been found to conform to a special RS CVn-type designation (Hall, 1976); Morgan and Eggleton, 1979). Svechnikov (1969) described these as AR systems. The issue will be discussed further in the next section. Sz Szafraniec (see (12) and (13) above.) Her gathered information on photometry is often of interest in connection with less well-known candidates. sd Semi-detached, in the sense of Kopal (1955). sec Secondary. tr Transit, i.e. eclipse formed by the smaller star obscuring the larger one. --- Julie Anne Watko SSDOO/ADC Francois Ochsenbein CDS 1996 Jun 11 V_46.xml A Catalogue of Field Type II Cepheids 5048 V/48 Field Type II Cepheids A Catalogue of Field Type II Cepheids H C Harris AJ 90 756 1985 1985AJ.....90..756H Stars, variable This catalog contains two data files of Type II Cepheids. The primary file consists of 152 Cepheids. These Cepheids are farther than 600 pc from the Galactic plane, and all of them are likely field Type II (low mass or Population II stars) Cepheids. The second file contains 56 additional stars that are likely, but more uncertainly, Type II Cepheids. These additional stars either have large Z distances but lack of reddening estimates or lie close to the Galactic plane identified as Type II base upon independent evidence (Petit 1960; Woolley 1966; Szabdos 1977; Wallerstein et al. 1979; Lloyd 1983; Harris et al 1984). Both of these two files have the same record format for each Cepheid. The format includes star name, equatorial (1900) and galactic coordinates, period, approximate mean magnitude, distance from the Sun and from the Galactic plane, computed reddening, and the most recent supplement to the General Catalog of Variable Stars (GCVS) where the star is listed.
Type II Cepheids ID Star (variable) name --- RAh Right ascension hours (1900) h RAm Right ascension minutes (1900) min RAs Right ascension seconds (1900) s DE- Sign of declination --- DEd Declination degrees (1900) deg DEm Declination minutes (1900) arcmin GLON Galactic longitude deg GLAT Galactic latitude deg per Period d mag Mean magnitude mag n_mag Code indicating type of magnitude P = photographic V = Johnson V B = Johnson B --- dist Distance from the sun kpc z_dist Distance from the galactic plane kpc E_B-V B-V color excess (reddening) mag n_E_B-V Code indicating source of E(B-V) d = From HI (Burstein and Heiles 1982) e = From field stars (Fernie and Hube 1968) --- supp Most recent GCVS listing star The most recent supplement as of 1985 --- Probable type II Cepheids based on |Z| distance ID Star (variable) name --- RAh Right ascension hours (1900) h RAm Right ascension minutes (1900) min RAs Right ascension seconds (1900) s DE- Sign of declination --- DEd Declination degrees (1900) deg DEm Declination minutes (1900) arcmin GLON Galactic longitude deg GLAT Galactic latitude deg per Period d mag Mean magnitude mag n_mag Code indicating type of magnitude P = photographic V = Johnson V B = Johnson B --- dist Distance from the sun kpc z_dist Distance from the galactic plane kpc E_B-V B-V color excess (reddening) mag supp Most recent GCVS listing star The most recent supplement as of 1985 --- N.G. Roman ADC/SSDOO 1997 Jul 22 V_48.xml The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version) 5050 V/50 Bright Star Catalogue, 5th Revised Ed. The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version) E D Hoffleit W H Warren Jr. Astronomical Data Center, NSSDC/ADC ??? ??? 1991 1991bsc..book.....H Combined data Stars, bright The Bright Star Catalogue (BSC) is widely used as a source of basic astronomical and astrophysical data for stars brighter than magnitude 6.5. The catalog contains the identifications of included stars in several other widely-used catalogs, double- and multiple-star identifications, indication of variability and variable-star identifiers, equatorial positions for B1900.0 and J2000.0, galactic coordinates, UBVRI photoelectric photometric data when they exist, spectral types on the Morgan-Keenan (MK) classification system, proper motions (J2000.0), parallax, radial- and rotational-velocity data, and multiple-star information (number of components, separation, and magnitude differences) for known nonsingle stars. In addition to the data file, there is an extensive remarks file that gives more detailed information on individual entries. This information includes star names, colors, spectra, variability details, binary characteristics, radial and rotational velocities for companion stars, duplicity information, dynamical parallaxes, stellar dimensions (radii and diameters), polarization, and membership in stellar groups and clusters. The existence of remarks is flagged in the main data file. The BSC contains 9110 objects, of which 9096 are stars (14 objects catalogued in the original compilation of 1908 are novae or extragalactic objects that have been retained to preserve the numbering, but most of their data are omitted), while the remarks section is slightly larger than the main catalog. The present edition of the compilation includes many new data and the remarks section has been enlarged considerably. This preliminary version of the fifth edition of the Bright Star Catalogue supersedes the published and machine-readable versions of Hoffleit (1982, Yale University Observatory) and is intended for use until the final version of this edition is completed. It has been made available only for dissemination on the Astronomical Data Center CD ROM. The brief format description applies to the preliminary version of the catalog only. The format will change for the final edition.
The main part of the Catalogue HR Harvard Revised Number = Bright Star Number number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- Name Name, generally Bayer and/or Flamsteed name number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- DM Durchmusterung Identification (zone in bytes 17-19) number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- HD Henry Draper Catalog Number number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- SAO SAO Catalog Number number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- FK5 FK5 star Number number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- IRflag I if infrared source number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- r_IRflag Coded reference for infrared source Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- Multiple Double or multiple-star code A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- ADS Aitken's Double Star Catalog (ADS) designation number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- ADScomp ADS number components number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- VarID Variable star identification number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- RAh1900 Hours RA, equinox B1900, epoch 1900.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). h RAm1900 Minutes RA, equinox B1900, epoch 1900.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). min RAs1900 Seconds RA, equinox B1900, epoch 1900.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). s DE-1900 Sign Dec, equinox B1900, epoch 1900.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). --- DEd1900 Degrees Dec, equinox B1900, epoch 1900.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). deg DEm1900 Minutes Dec, equinox B1900, epoch 1900.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). arcmin DEs1900 Seconds Dec, equinox B1900, epoch 1900.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). arcsec RAh Hours RA, equinox J2000, epoch 2000.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). h RAm Minutes RA, equinox J2000, epoch 2000.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). min RAs Seconds RA, equinox J2000, epoch 2000.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). s DE- Sign Dec, equinox J2000, epoch 2000.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). --- DEd Degrees Dec, equinox J2000, epoch 2000.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). deg DEm Minutes Dec, equinox J2000, epoch 2000.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). arcmin DEs Seconds Dec, equinox J2000, epoch 2000.0 number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). arcsec GLON Galactic longitude number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). deg GLAT Galactic latitude number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). deg Vmag Visual magnitude number=1 These fields are all blanks for stars removed from the Bright Star Catalogue (see notes.dat). mag n_Vmag Visual magnitude code blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- u_Vmag Uncertainty flag on V number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- B-V B-V color in the UBV system number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. mag u_B-V Uncertainty flag on B-V number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- U-B U-B color in the UBV system number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. mag u_U-B Uncertainty flag on U-B number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- R-I R-I in system specified by n_R-I number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. mag n_R-I Code for R-I system (Cousin, Eggen) number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- SpType Spectral type number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- n_SpType Spectral type code number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- pmRA Annual proper motion in RA J2000, FK5 system number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. arcsec/yr pmDE Annual proper motion in Dec J2000, FK5 system number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. arcsec/yr n_Parallax D indicates a dynamical parallax, otherwise a trigonometric parallax number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- Parallax Trigonometric parallax (unless n_Parallax) number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. arcsec RadVel Heliocentric Radial Velocity number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. km/s n_RadVel Radial velocity comments V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- l_RotVel Rotational velocity limit characters number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- RotVel Rotational velocity, v sin i number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. km/s u_RotVel uncertainty and variability flag on RotVel number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- Dmag Magnitude difference of double, or brightest multiple number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. mag Sep Separation of components in Dmag if occultation binary. number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. arcsec MultID Identifications of components in Dmag number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- MultCnt Number of components assigned to a multiple number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- NoteFlag a star indicates that there is a note (file notes.dat) number= Blank if from NASA merged Infrared Catalogue, Schmitz et al., 1978; ' if from Engles et al. 1982 : if uncertain identification number= A = Astrometric binary D = Duplicity discovered by occultation; I = Innes, Southern Double Star Catalogue (1927) R = Rossiter, Michigan Publ. 9, 1955 S = Duplicity discovered by speckle interferometry. W = Worley (1978) update of the IDS; number= blank = V on UBV Johnson system; R = HR magnitudes reduced to the UBV system; H = original HR magnitude. number= V = variable radial velocity; V? = suspected variable radial velocity; SB, SB1, SB2, SB3 = spectroscopic binaries, single, double or triple lined spectra; O = orbital data available. --- Remarks HR Harvard Revised (HR) number= the following abbreviations are used: C - Colors; D - Double and multiple stars; DYN - Dynamical parallaxes; G - Group membership; M - Miscellaneous. N - Star names; P - Polarization; R - Stellar radii or diameters; RV - Radial and/or rotational velocities; S - Spectra; SB - Spectroscopic binaries; VAR - Variability; The category abbreviation is always followed by a colon (:). --- Count Note counter (sequential for a star) number= the following abbreviations are used: C - Colors; D - Double and multiple stars; DYN - Dynamical parallaxes; G - Group membership; M - Miscellaneous. N - Star names; P - Polarization; R - Stellar radii or diameters; RV - Radial and/or rotational velocities; S - Spectra; SB - Spectroscopic binaries; VAR - Variability; The category abbreviation is always followed by a colon (:). --- Category Remark category abbreviation: the following abbreviations are used: C - Colors; D - Double and multiple stars; DYN - Dynamical parallaxes; G - Group membership; M - Miscellaneous. N - Star names; P - Polarization; R - Stellar radii or diameters; RV - Radial and/or rotational velocities; S - Spectra; SB - Spectroscopic binaries; VAR - Variability; The category abbreviation is always followed by a colon (:). number= the following abbreviations are used: C - Colors; D - Double and multiple stars; DYN - Dynamical parallaxes; G - Group membership; M - Miscellaneous. N - Star names; P - Polarization; R - Stellar radii or diameters; RV - Radial and/or rotational velocities; S - Spectra; SB - Spectroscopic binaries; VAR - Variability; The category abbreviation is always followed by a colon (:). --- Remark Remarks in free form text number= the following abbreviations are used: C - Colors; D - Double and multiple stars; DYN - Dynamical parallaxes; G - Group membership; M - Miscellaneous. N - Star names; P - Polarization; R - Stellar radii or diameters; RV - Radial and/or rotational velocities; S - Spectra; SB - Spectroscopic binaries; VAR - Variability; The category abbreviation is always followed by a colon (:). --- Francois Ochsenbein CDS 1995 Nov 02 Author's addresses: Dorrit Hoffleit Department of Astronomy Yale University Wayne H. Warren Jr. ST Systems Corporation National Space Science Data Center NASA Goddard Space Flight Center UNKNOWN UNKNOWN * 02-Oct-1993 at CDS (Francois Ochsenbein) A few corrections have been inserted from the CD-ROM version "Selected Astronomical Catalogs, Volume 1, 1991, directory /combined/bsc5 at CDS with the agreement of Wayne H. Warren Jr: 1. The spectral type for HR 6397 is from Walborn and contained octal 032 (control-Z) characters instead of square brackets around the "n". 2. Two remarks have been added for 6985 and 8817 3. Byte 197 (NoteFlag) of "catalog" file corrected for stars 202 7126 7482 7614 8982 (removed asterisk) 285 342 841 843 991 1181 1553 1652 2269 2271 (added asterisk) 2837 3133 3962 4522 4789 6692 7076 7328 8306 8667 (added asterisk) * 02-Nov-1995 at CDS (Francois Ochsenbein): Documentation slightly changed to accommodate to standards, and two lines which were inverted in "notes" have been replaced. V_50.xml Data Inventory of Space-Based Celestial Observations, Version 1.1 5051 V/51 Data Inventory of Space-Based Obs, Ver 1.1 Data Inventory of Space-Based Celestial Observations, Version 1.1 L E Brotzman R S Hill J M Mead ADC Bull. 1 312 1987 1987 References Space observations The "Data Inventory of Space-Based Celestial Observations Version 1.0" (DISCO) is a directory to data contained in sixteen catalogs dealing with observations from space. (Sounding rocket, solar, and planetary observations have been excluded.) The information extracted from the catalogs includes names of objects observed, 1950 equatorial coordinates, and the name of the catalog or instrument. A second file contains full references to the source catalogs and other pertinent information. The purpose of creating DISCO is (1) to unify astronomical observations from space, which are at present scattered and hard to locate, and then (2) to provide a machine-readable index to these observations, thus enabling easy access by computer. Such a directory will permit an astronomer to find out what objects have been observed from space, which spacecraft and instruments made the observations, and where to go to find the data themselves.
Catalog Data PID Primary or "mission" id Space is provided for three object identifiers. The identifiers are listed according to the following priority: (1) "Mission id", (2) HD or NGC, (3) other. Namely, (1) Primary id, (2) Secondary, and (3) Tertiary id. --- SID Secondary id --- TID Tertiary id --- RAh RA hours Equatorial coordinates, equinox 1950.0. Some of the original catalogs do not have coordinates, in which case coordinates have been obtained from a standard ground-based catalog. See coord reference below. h RAm RA minutes min RAs RA seconds s RAp RA precision RA precision. Number of digits HH MM SS.SS given in the source catalog; for example, 6 is the code for whole numbers of seconds. --- DE- Sign of dec --- DEdeg Dec degrees deg DEm Dec arc minutes arcmin DEs Dec arc seconds arcsec DEp Dec precision DEC precision. Number of digits DD MM SS.SS given in the source catalog; for example, 8 is the code for hundredths of seconds. --- CRefNum Coordinate reference number Coord reference. Reference number for the source of coordinates, as given in the reference file; see refs.dat. --- Cat Mission or catalog Mission or catalog. Identification of the satellite or instrument that observed the object or the name of the catalog from which the data were taken. --- PRefNum Primary reference number Primary reference. Reference number for the primary source of information, as given in the reference file; see refs.dat below. --- References RefNum Reference number Reference number. The number given the catalog when compiled into the DISCO. If this field is blank, the record is a continuation of the previous record. If the reference number is greater than or equal to 100, the refer- enced catalog was used only to find coordinates of objects. --- StatNum ADC Status Report number Status Report no. The number under which the catalog may be located in the ADC Status Report. --- SCAbbr Satellite or catalog abbrev. This is the abbreviation given the satellite or catalog by ADC personnel. --- Rcount Record count Record count. The number of records from this reference that can be found in DISCO. --- Ref Reference Reference. This field includes the full title and reference of the original paper that presented the data; or the name of a catalog used for coordinates only if the reference number is greater than 100 (see above). See the description for bytes 75-78 and 115-118 in disco.dat. --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Aug 16 UNKNOWN UNKNOWN The ReadMe file incorporates the original ADC documentation by Brotzman, Hill, and Mead (1986). "The Data Inventory of Space-Based Celestial Observations" (DISCO) was produced at the Astronomical Data Center (ADC), NASA Goddard Space Flight Center. A search through the ADC Status Report was conducted for all catalogs containing data from satellite observations. Individual Fortran programs were written that produced a DISCO "submaster" from each catalog. The submasters were then merged and sorted by equatorial coordinates. In some cases, the input catalogs were edited with Fortran programs or a text editor to produce a preliminary dataset that was more amenable to conversion to DISCO format. In addition, coordinates were obtained from ground-based catalogs for objects that do not have them in the original space-based lists (see the description of the coordinate reference in "Main Inventory File disco.dat above). Complete versions of the catalogs represented in DISCO are available from the ADC. V_51.xml Catalogue of the brightest stars 5053 V/53 Catalogue of the Brightest Stars Catalogue of the brightest stars F Ochsenbein J L Halbwachs Bull. Inform. CDS 32 83 1987 1987BICDS..32...83O Catalogue of the brightest stars F Ochsenbein A Acker E Legrand J M Poncelet E Thuet-Fleck A.Acker ed., Strasbourg Obs. ??? ??? 1988 1988 V/50 : The Bright Star Catalogue, 5th Edition Hoffleit D. 1982, "The Bright Star Catalogue", 4th Edition (in collaboration with C. Jaschek), Yale Observatory (catalog <V/25>) Ochsenbein F., Acker A., Legrand E., Poncelet J.M., and Thuet-Fleck E. 1984, "Catalogue des Etoiles les Plus Brillantes", ed. Acker A., Observatoire de Strasbourg, Centre de Donnees astronomiques et Planetarium de Strasbourg Lanz T. =1986A&AS...65..195L (catalog <II/116>) Stars, bright Combined data This catalogue provides data on the 1628 stars brighter than magnitude 5.01 contained in the "catalogue des etoiles les plus brillantes" by Ochsenbein et al. (1984), compiled from the fourth edition of The Bright Star Catalogue (Hoffleit 1982). It differs from the original printed version by the following points: - ecliptic coordinates were added to astrometric data - UBVRI photometry was taken from Lanz (1986); for that reason, three stars (HR 3229, HR 4392 and HR 6161) are fainter than 5 mag. Moreover, the blanks due to unknown indices were filled with the value 99.99 (or 99.999 for the uvbyHbeta photometry). - the greek letter "delta" that appears in some spectral types is now written in latin letters instead of the code "<04>". - the luminosity classes are coded as integer numbers in an additional column. - the number of components of visual double stars is given.
Ce catalogue fournit des donnees sur les 1628 etoiles brillantes de magnitude allant jusqu'a 5.01 contenues dans le "catalogue des etoiles les plus brillantes" de F. Ochsenbein et co. (1984), lui-meme derive de la 4eme edition du "Bright Star Catalogue" (Hoffleit 1982). Il differe de la version originale imprimee par les points suivants: - les coordonnees ecliptiques ont ete ajoutees aux donnees astrometriques. - la photometrie UBVRI a ete extraite du catalogue de Lanz (1986); ceci explique que trois etoiles soient de magnitude superieure a 5.00 (HR 3229, HR 4392 et HR 6161). De plus, afin de faciliter les traitements par programme, on donne la valeur 99.99 en cas de mesure manquante (99.999 pour l'uvbyHbeta). - la lettre grecque "delta", qui apparaissait dans les types spectraux sous la forme codee "<04>" est maintenant ecrite en toutes lettres. - une colonne donnant la classe de luminosite en chiffre arabe a ete ajoutee a l'ecriture classique du type spectral. - le nombre de composantes des etoiles doubles visuelles (2) est donne explicitement.
The Catalogue HR "Bright Star" catalog <V/50> --- HD Henry Draper" catalog <III/135> --- Flamsteed Flamsteed number --- Bayer Greek letter (lettre grecque) --- Const Constellation (3 characters) --- VarName Designation as Variable Star --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec precRA Precession in RA for 10 years 0.1s/a precDE Precession in DE for 10 years 0.1arcsec/a ELON Ecliptic longitude deg ELAT Ecliptic latitude deg GLON Galactic longitude deg GLAT Galactic latitude deg pmRA Proper motion (mouvement propre) in RA number=7 Proper motion contains the cos(DE) term (ce mouvement propre est la variation annuelle de RA * cos(DE)) arcsec/a pmDE Proper motion (mouvement propre) in DE arcsec/a RVel Radial velocity (vitesse radiale) km/s n_RVel Comment on RVel number=3 Note on RVel: V: variable velocity without known reason (vitesse variable sans raison determinee) SB: spectroscopic binary (binaire spectroscopique) SB1: one-spectrum binary (binaire a un spectre) SB2: two visible spectra (le deuxieme spectre est visible) O: known orbit (les elements orbitaux ont ete determines) --- n_Plx "D" when Plx is a dynamical parallax ("D" si la parallaxe qui suit est dynamique) --- Plx Parallax, trigonometric or dynamic (see n_Plx) number=1 Field may be blank (la donnee peut etre inexistante) arcsec Vmag Visual magnitude (magnitude visuelle) mag B-V B-V (Johnson) index number=2 The value 99.99 or 99.999 indicates an unknown value (la valeur 99.99 ou 99.999 indique l'inexistance de la donnee) mag U-B U-B (Johnson) index number=2 The value 99.99 or 99.999 indicates an unknown value (la valeur 99.99 ou 99.999 indique l'inexistance de la donnee) mag V-R V-R (Johnson) index number=2 The value 99.99 or 99.999 indicates an unknown value (la valeur 99.99 ou 99.999 indique l'inexistance de la donnee) mag R-I R-I (Johnson) index number=2 The value 99.99 or 99.999 indicates an unknown value (la valeur 99.99 ou 99.999 indique l'inexistance de la donnee) mag b-y Stromegren index number=2 The value 99.99 or 99.999 indicates an unknown value (la valeur 99.99 ou 99.999 indique l'inexistance de la donnee) mag m1 Stroemgren index number=2 The value 99.99 or 99.999 indicates an unknown value (la valeur 99.99 ou 99.999 indique l'inexistance de la donnee) mag c1 Stroemgren index number=2 The value 99.99 or 99.999 indicates an unknown value (la valeur 99.99 ou 99.999 indique l'inexistance de la donnee) mag Hbeta Stroemgren index number=2 The value 99.99 or 99.999 indicates an unknown value (la valeur 99.99 ou 99.999 indique l'inexistance de la donnee) mag l_vsini Limit flag for vsini number=4 The ':' in the flag n_vsini stands for "less or equal" (le symbole ':' signifie "inferieur ou egal") --- vsini Projected rotational velocity (projection de la vitesse de rotation sur la ligne de visee) number=1 Field may be blank (la donnee peut etre inexistante) km/s u_vsini ':' for uncertainty (marque d'incertitude) --- Wgamma Equivalent width of H-gamma line (largeur equivalente de la raie Hgamma) (en Angstroem = 10-10m) number=1 Field may be blank (la donnee peut etre inexistante) 0.1nm WilsonLC Wilson Luminosity Class number=5 only present when MK luminosity class absent (uniquement lorsque le type MK n'est pas complet) --- SpType MK Spectral Type --- LClass Numeric Luminosity Class (classe de luminosite exprimee en chiffre) number=1 Field may be blank (la donnee peut etre inexistante) --- nComp Number of visual components (nombre de composantes visuelles) --- Dmag Magnitude difference between components (difference de magnitude entre les composantes) Comp number=1 Field may be blank (la donnee peut etre inexistante) mag Sep Separation between Comp number=1 Field may be blank (la donnee peut etre inexistante) arcsec Comp Designation of components number=6 Designation of components concerned by columns Dmag and Sep (Designation des composantes concernees par Dmag et Sep); "O" designates a binary discovered by occultation methods (binaire decouverte par occultation) --- Francois Ochsenbein CDS 1996 May 31 V_53.xml A catalogue of high-velocity stars 5055 V/55 A catalogue of high-velocity stars A catalogue of high-velocity stars N G Roman Astrophys. J. Suppl. 2 195 1955 1955ApJS....2..195R Stars, high-velocity RHV catalogue on magnetic tape was prepared in process of compilation of population II stars catalogue on magnetic tape (Pop2) at Astrophysical Department, Insitute of Physics, Lithuanian Academy of Sciences, under supervision of A. Bartkevicius. Printed version of RHV catalogue contains 633 nonvariable high-velocity stars north of Dec -20 degrees, brighter than 9.5 mvis. A detailed information on RHV catalogue is given in original publication RHV catalogue on magnetic tape contains some modifications and additions: 1. Stars from tables 1 and 2 are sorted according to RA (1950.0) in the same file. 2. In addition to original equatorial coordinates RA, Dec (1900.0), there are presented RA, Dec (1950.0, 1875.0, 1855.0), RA, Dec (1950.0) in radians, and galactic coordinates (l, b). 3. HD number is given instead of Flamsteed number or Bayer designation. 4. MDSP and MDSPS1 numbers in catalogues of metal-deficient stars (A. Bartkevicius, Bull. Vilnius Obs., No.51, 1980; No.68, 1984) are added. The author, N. Roman, discovered an error in the printed catalog in the correction for solar motion. She corrected this error and recomputed the orbital elements.
High-velocity stars catalogue RHV RHV catalogue number --- Note P indicates that the star is from Table 2 --- Name HD/BD Number --- n_Name Binary star component --- MDSP/S1 MDSP/S1 Catalogue Number --- n_MDSP/S1 P indicates the MDSPS1 --- RAh Right ascension 1900.0 h RAm Right ascension 1900.0 min DE- Declination sign --- DEd Declination 1900.0 deg DEm Declination 1900.0 arcmin RAh2 Right ascension 2000.0 h RAm2 Right ascension 2000.0 min DE-2 Declination sign --- DEd2 Declination 2000.0 deg DEm2 Declination 2000.0 arcmin RArad Right ascension 1950.0 rad DErad Declination 1950.0 rad GLON Galactic longitude l deg GLAT Galactic latitude b deg n_Spect M indicates a spectrum from Johnson and Morgan (1953) --- Spect Spectrum --- n_Vmag J indicates UBV photometry from Johnson & Morgan(1953) --- Vmag V magnitude mag u_Vmag rms uncertainty on Vmag --- B-V B-V color-index mag u_B-V rms uncertainty on B-V --- U-B U-B color-index mag u_U-B rms uncertainty on U-B --- plx Trigonometric parallax arcsec SpPlx Spectroscopic parallax arcsec RV Radial velocity km/s pmRA Proper motion in right ascension arcsec/yr pmDE Proper motion in declination arcsec/yr Spm Source of the proper motion --- Uvel U component of space motion (L=90.0, B=0) km/s Vvel V component of space motion (L=180.0, B=0) km/s Wvel W component of space motion (B=0, + to N) km/s Vel Total space velocity km/s eps Eccentricity of the Newtonian orbit --- a Semimajor axis of the orbit (99.9 if >99.9) kpc n_Vel R indicates retrograde motion --- Notes * indicates a note in file notes --- Notes RHV RHV catalogue number --- Note p indicates that the star is from Table 2 --- Name HD or BD number --- Rem Remarks --- Patricia Bauer CDS 1994 Nov 30 V_55.xml The Catalogue of Metallicities, Velocity Components and Orbital Parameters for F2-K5 Dwarfs in the Vicinity of 80 pc from the Sun 5058 V/58 [Fe/H], Vel, Orbits, F2-K5 Dwarfs 80pc from Sun The Catalogue of Metallicities, Velocity Components and Orbital Parameters for F2-K5 Dwarfs in the Vicinity of 80 pc from the Sun V A Marsakov Yu G Shevelev CDS Inf. Bull. 35 129 1988 1988BICDS..35..129M Abundances, [Fe/H] Space velocities Stars, late-type In this catalog, metallicities, distances, components of space velocities and parameters of osculating orbits are calculated for 1065 F2-K5 dwarfs with UBV photometric data, proper motions and radial velocities. The present sample is composed on the base of the Ochsenbein (1980) catalogue and contains the stars of the V (IV-V) luminosity class, within the colour range 0.35<B-V<1.10 (which corresponds to the spectral class range F2-K5). Sandage's (1969) Hyades sequence was used to determine the value delta (U-B) for each star. The authors calibrated the ultraviolet excess in terms of FE/H! separately for the four of the temperature index (B-V) where delta(U-B) practically does not depend on the effective temperature. Intervals in (B-V) correspond to the following division on spectral class intervals: F2-F9, G0-G4, and G5-G9, K0-K5. Metallicity is calculated from the formulae: FE/H!=-5.3*delta(U-B)+0.02 for stars F2-F9 FE/H!=-5.1*delta(U-B)+0.13 for stars G0-G4 FE/H!=-5.4*delta(U-B)+0.02 for stars G5-G9 FE/H!=-4.7*delta(U-B)-0.04 for stars K0-K5 These relations follow from the assumption that mean metallicity and metallicity dispersion for stars of all spectral classes are the same. Distances to the stars were calculated from spectral parallaxes. Absolute magnitudes (M(V)) were obtained from the Sp,M(V)-relation for dwarfs (Straizys, 1982). The sample includes only stars nearer than 80 pc because reddening is negligible for them. the obtained distances together with radial velocities and proper motions are used to calculate the components of space velocities. The eccentricities, apogalactic and perigalactic distances of the stars were calculated from the osculating orbit approximation according to the galaxy model from the paper by Eggen et al. (1962).
Catalog file HD HD number --- GLON Galactic longitude deg GLAT Galactic latitude deg V Brightness in V filter mag B-V B-V color index mag U-B U-B color index mag Sp Spectral type --- R Heliocentric distance pc Uvel Velocity vector component in the direction of the anticenter of the Galaxy km/s Vvel Velocity component in the direction of Galactic rotation km/s Wvel Velocity component towards the north Galactic pole km/s R1 Apogalactic distance of the Galactic orbit kpc R2 Perigalactic distance of the Galactic orbit kpc e Eccentricity of the Galactic orbit --- E(U-B) Ultraviolet excess mag FE/H! Metallicity (FE/H!=LG(FE/H)(star)-LG(FE/H)(sun)) --- desc.doc Author's documentation James E. Gass SSDOO/ADC 1997 Sep 09 V_58.xml Catalogue of Cataclysmic Binaries, Low-Mass X-Ray Binaries and Related Objects 5th edition 5059 V/59 Cataclysmic Bin, Low-Mass X-ray Bin, Related obj Catalogue of Cataclysmic Binaries, Low-Mass X-Ray Binaries and Related Objects 5th edition H Ritter Astron. Astrophys. Suppl. Ser. 85 1179 1990 1990A&AS...85.1179R V/82 : compilation of cataclysmic binaries with known or suspected orbital periods (Ritter H., Kolb U., in "X-ray Binaries", Cambridge Astrophys. Ser. No 26) to previous editions: Ritter, H.: 1982, preprint, Max-Planck-Institut fuer Physik und Astro- physik, MPA 22 (1st Edition, June 1982) Ritter, H.: 1983, preprint, Max-Planck-Institut fuer Physik und Astro- physik, MPA 51 (2nd Edition, January 1983) Ritter H., 1984, A&AS 57, 385 (3rd edition) (Catalogue: V/37) Ritter H., 1987, A&AS 70, 335 (4th edition) Wanted by the author: References to accurate coordinates and published finding charts for objects listed below. data published in easily accessible journals, cata- logues and circulars, such as Acta Astron., Astron. Astrophys., Astron. J., Astrophys. J., Monthly Notices Roy. Astron. Soc., Nature, Publ. Astron. Soc. Pacific, IAU Circ., Inf. Bull. Variable Stars, etc. are strongly preferred. the requested data are needed to improve and supple- ment future editions of this catalogue. if you know where the data in question have been published, please send the data and the corresponding references (or only the references) to Dr. Hans Ritter Max-Planck-Institut fuer Physik und Astrophysik Karl-Schwarzschild-Strasse 1 D-8046 Garching Germany Accurate coordinates are needed for the following objects: HV AND DM DRA CY UMA CV IN M 67 MS1603+2600 AT CNC CP ERI BPM 71214 LB 1800 The accuracy of the coordinates of the following objects is either worse than 5 seconds of arc or unknown. Improved or confirmed coordinates are therefore desirable. V1315 AQL V664 CAS BR LUP DW UMA LMC X-2 PG1026+002 V1405 AQL V442 CEN FY PER EI UMA SP 1 4U1624-49 WX ARI V803 CEN AY PSC RW UMI PG0308+096 4U1702-36 CR BOO BW CIR QR SGE SS UMI H0534-581 4U1705-44 RR CAE TX COL V4140 SGR GK VIR 1E0547-7109 BY CAM BL HYI NN SER QQ VUL 1H0709-36 QU CAR DO LEO BE UMA GRU V1 PG0818+513 References to published finding charts, wherever possible photographic ones, are needed for the following objects: BW CIR CY UMA CV IN M 67 L870-2 MS1603+2600 1H1929+509 DM DRA BPM 71214 LB 1800 1H0709-36 References to better, i.e. photographic, finding charts would be welcome for the following objects: HV AND AT CNC V425 CAS IP PEG FY PER Binaries, cataclysmic Binaries, X-ray The catalogue lists coordinates, magnitudes, orbital parameters, stellar parameters of the components and other characteristic properties of 168 cataclysmic binaries, 36 low-mass X-ray binaries and 28 related objects with known or suspected orbital periods together with a comprehensive selection of the relevant literature that appeared after 1986. In addition the catalogue contains a list of references to published finding charts for 222 of the 232 objects. A cross-reference list of object designations concludes the catalogue.
The objects listed in this catalogue are subdivided into three main object classes, i.e. into "Cataclysmic Binaries", "Low-Mass X-Ray Binaries" and "Related Objects" The defining characteristics of the three object classes used here are the following: c a t a c l y s m i c b i n a r i e s Are semi-detached binaries consisting of a white-dwarf primary (or a white-dwarf precursor) and a low-mass secondary which is filling its critical roche lobe. The secondary need not necessarily be un- evolved. It may even be a highly evolved star as e.g. in the cases of GP COM and AM CVN. A more detailed description of the main char- acteristics of these objects may be found in the following books and review articles: Bode, M.F., Evans, A., (Eds.): 1989, Classical Novae, John Wiley & Sons ltd., Chichester Cropper,M.: 1990, Space Sci. Rev., in press (for the Am Her stars) la Dous, C.: 1990, in: Cataclysmic Variables and Related Objects, M. Hack, (Ed.), NASA / CNRS Monograph Series on Non-Thermal Phenomena in Stellar Atmospheres, in press Wade, R. A.: 1985, in: Interacting Binaries, P. P. Eggleton and J. E. Pringle (Eds.), D. Reidel Publ. Co., Dordrecht Wade, R.A., Ward, M.J.: 1985, in: Interacting Binary Stars, J.E. Pringle and R.A. Wade (Eds.), Cambridge Univ. Press, p. 129 Warner, B.: 1976, in: Structure and Evolution of Close Binary Sys- tems, IAU Symp. no. 73, P. Eggleton, S. Mitton and J. Whelan (Eds.), D. Reidel (Dordrecht), p. 85 l o w - m a s s x - r a y b i n a r i e s Are semi-detached binaries consisting of a neutron-star primary and a low-mass secondary which is filling its critical roche lobe. Observationally they are distinguished from the luminous massive X-ray binaries by the following main properties: in general the spectra of the low-mass x-ray binaries (at maximum light) are devoid of normal stellar absorption features. The ratio of their X-ray to optical luminosities is much larger than unity. Typically it ranges from about 100 to about 10000. A more detailed descript- ion of the main characteristics of these objects may be found in the following review articles: Mason, K.O.: 1986, in: Physics of Accretion onto Compact Objects, Lecture Notes in Physics, Vol. 266, K.O. Mason, M.G. Watson, and N.E. White (Eds.), Springer Verlag, Heidelberg, p. 29 Mc McClintock, J.E., Rappaport, S.A.: 1985, in: Cataclysmic Variab- les and Low-Mass X-Ray Binaries, D.Q. Lamb and J. Patterson, (Eds.),D. Reidel Publ. Co., Dordrecht, p. 61 White, N.E., Mason, K.O.: 1985, Space Science Reviews 40, 167 R e l a t e d O b j e c t s Are detached binaries consisting of a white dwarf primary (or a white dwarf precursor) and a low-mass secondary which is detached from its critical roche lobe. The secondary may also be a highly evolved star. for a review see e.g. Bond, H.E.: 1985, in: Cataclysmic Variables and Low-Mass X-ray Binaries, D.Q. Lamb and J. Patterson (eds.), D. Reidel, Dord- recht, p.15 Bond, H.E.: 1989, in: Planetary Nebulae, S. Torres-Peimbert (ed.), Kluwer, Dordrecht, p. 251 Ritter, H.: 1986, Astron. Astrophys. 169, 139 According to the subdivision in these three object classes the catalogue contains three major sections. Each of the three catalogue sections is further subdivided into a catalog file, where a few characterizing parameters of the object are tabulated, and into a reference file, where a selection of refer- ences is given. Within each of the sections, the objects are listed in order of decreasing orbital period. In the corresponding re- ference section, however, the objects are listed in lexigraphical order. The quantities listed in the catalog file and the corresponding abbreviations used in the table headings are described in the notes to the byte by byte descriptions below. The catalogue is supplemented by a list giving references to published finding charts (fc) of the objects. In this file the objects of all three classes are merged and listed in lexigraphical order. In order to facilitate finding a particular object, two lists of the objects catalogued are given. The first list gives the objects in lexigraphical order, the second one in order of increasing right ascension. For each object, both lists give three page numbers for the printed file catalog.doc: the first one referring to the table section (ts), the second one to the corresponding reference section (rs) and the third one to the list giving references to the finding charts (fc). An asterisk following the name of the object indicates that the object is also known under other designations. these are cross-referenced in the "who's who ?" (whoswho.dat) file. This file includes also a list of references to various catalogue acronyms that appear in this compilation. A more complete list of this kind may be found in "the first dictionary of the nomenclature of celestial objects" by A. Fernandez, M.-C. Lortet and F. Spite that appeared in Astron. Astrophys. Suppl. Ser. 52, Vol. 4, (1983) and in its supplements by M.-C. Lortet in Astron. Astrophys. Suppl. Ser. 64, 303-324, 325-328 (1986) and by M.-C. Lortet and F. Spite in Astron. Astrophys. Suppl. Ser. 64, 329-390 (1986).
Catalog of cataclysmic binaries OBJECT Object name Object name : wherever possible, the designation of the object given in the general catalogue of variable stars is used here. --- Alt Alternative name Alternate name : Is a frequently used alternative name. Further alternative designations are given in the whoswho.dat file. --- RAh Right Ascension J2000 hours Coordinates : Right ascension (2000.0) in hrs min sec Declination (2000.0) in deg ' " the coordinates are given in the following format: right ascension: hh mm ss.s declination : ddd mm ss a h RAm RA J2000 minutes Coordinates : Right ascension (2000.0) in hrs min sec Declination (2000.0) in deg ' " the coordinates are given in the following format: right ascension: hh mm ss.s declination : ddd mm ss a min RAs RA J2000 seconds Coordinates : Right ascension (2000.0) in hrs min sec Declination (2000.0) in deg ' " the coordinates are given in the following format: right ascension: hh mm ss.s declination : ddd mm ss a s DE- Sign Declination J2000 --- DEd Declination J2000 Degrees deg DEm Declination J2000 arc minutes arcmin DEs Declinations J2000 arc seconds arcsec CoordAcc Accuracy of the coordinates, in hexadecimal number (A=10") In the declination field, "a" is the accuracy of of the coordinates in seconds of arc (written as a hexadecimal number, i.e. 10" = A , 11" = B , 12" = C , 13" = D , 14" = E , 15" = F). In a case where "A" > 15" or where the accuracy of the coordinates is not known, the "CoordAcc" field is left blank. --- OType1 first object type characterization The object type is coarsely characterized using the following abbreviations: AC = AM CVN STAR, DOES NOT CONTAIN HYDROGEN, SUBTYPE OF NL AM = POLAR = AM HER SYSTEM, SUBTYPE OF NL, CONTAINS A SYNCHRONOUSLY ROTATING, MAGNETISED WHITE DWARF CP = COHERENT PULSATOR, CONTAINS A COHERENTLY PULSATING WHITE DWARF DD = SYSTEM CONSISTS OF TWO DEGENERATE COMPONENTS DN = DWARF NOVA DQ = INTERMEDIATE POLAR OR DQ HER SYSTEM, CONTAINS A NON-SYNCHRONOUSLY ROTATING MAGNETISED WHITE DWARF DS = DETACHED SYSTEM N = CLASSICAL NOVA NA = FAST NOVA (DECLINE FROM MAX. BY 3 MAG. IN LESS THAN ABOUT 100 DAYS) NB = SLOW NOVA (DECLINE FROM MAX. BY 3 MAG. IN MORE THAN ABOUT 100 DAYS) NC = EXTREMELY SLOW NOVA (TYPICAL TIME SCALE OF THE DECLINE FROM MAXIMUM: DECADES) NL = NOVA-LIKE VARIABLE NR = RECURRENT NOVA PN = CENTRAL STAR OF A PLANETARY NEBULA SU = SU UMA STAR, SUBTYPE OF DN UG = DWARF NOVA OF EITHER U GEM OR SS CYG SUBTYPE UX = UX UMA STAR, SUBTYPE OF NL VY = VY SCL STAR (ANTI DWARF NOVA), SUBTYPE OF NL XB = X-RAY BURST SOURCE XL = LOW-MASS X-RAY BINARY, SCO X-1-LIKE XP = X-RAY PULSAR XS = X-RAY SOURCE XT = TRANSIENT X-RAY SOURCE ZC = Z CAM STAR, SUBTYPE OF DN * = OBJECT POSSIBLY RELATED TO THE DQ HER STARS --- u_OType1 uncertainty flag on OType1 --- OType2 second object type characterization --- u_OType2 uncertainty flag on OType2 --- OType3 third object type characterization --- OType4 fourth object type characterization --- l_mag1 limit on mag1 may be ">" or "<" --- mag1 magnitude Apparent V magnitude (B magnitude if followed by B) with the following meaning: mag1 = maximum brightness of NOVAE (N,NA,NB,NC,NR) IN MINIMUM DN (UG,ZC,SU) IN MINIMUM NL (UX,AC) IN NORMAL STATE NL (AM,VY) IN HIGH STATE XL (XT,XB) IN QUIESCENCE DS OUTSIDE ECLIPSE mag2 = minimum brightness, in case of eclipses magn. at mideclipse, of NOVAE (N,NA,NB,NC,NR) IN MINIMUM DN (UG,ZC,SU) IN MINIMUM NL (UX,AC) IN NORMAL STATE NL (AM,VY) IN HIGH STATE XL (XB,XT) IN QUIESCENCE DS mag3 = maximum brightness of NOVAE (N,NA,NB,NC,NR) IN OUTBURST DN (UG,ZC) IN OUTBURST DN (SU) IN NORMAL OUTBURST NL (AM,VY) IN LOW STATE XL (XB,XT) IN OUTBURST mag4 = brightness of ZC IN STANDSTILL SU IN SUPEROUTBURST = minimum brightness of NL (AM,VY) IN LOW STATE mag n_mag1 a "B" means that the magnitude is blue (visual otherwise) --- l_mag2 limit on mag2 may be ">" --- mag2 magnitude --- n_mag2 a "B" means that the magnitude is blue (visual otherwise) --- l_mag3 limit on mag3 may be ">" --- mag3 magnitude mag n_mag3 a "B" means that the magnitude is blue (visual otherwise) a "?" or ":" means that the value is uncertain --- l_mag4 limit on mag4 may be ">" --- mag4 magnitude mag n_mag4 a "B" means that the magnitude is blue (visual otherwise) a ":" means that the value is uncertain --- T1 Typical time interval between outbursts (in days) or minimum value for DN (UG, ZC), the typical time interval (in days) between two subsequent outbursts for DN (SU), the typical time interval (in days) between two subsequent normal outbursts for XL (XT), the typical time interval (in days) between two subsequent X-ray active states d n_T1 may be ":" or "-", when a maximum value T1max is available --- T1max maximum value of T1 d T2 typical time interval between two subsequent superoutbursts (in days) For DN (SU), the typical time interval (in days) between two subsequent superoutbursts d n_T2 may be "?" --- PerOrb Orbital period, in days Orbital period (in days), in case of object type DQ : the spectroscopic period is given here if it is different from the photometric one. SU : if followed by *, the orbital period has been estimated from the known superhump period using the empirical relation given by B. Stolz and R. Schoembs (1984,Astron.Astrophys.132,187) * : Spectroscopic Period, Photometric Period if followed by P. d n_PerOrb a ":" means uncertain value, and a "*" means spectroscopic period a "P" means photometric period --- P2 Second period, in days Second period (in days), in case of object type N, NA, NB, NC : orbital period of the prenova, unless the object is also of type DQ or *. In these cases see below. DQ : the photometric period is given here if it is different from the spectroscopic one. SU : superhump period. wherever possible, the super- hump period at the beginning of a superoutburst is given. * : photometric period. d u_P2 a ":" means uncertain value --- P3 Additional periods: third period Additional periods in the system (in seconds), in case of object type CP : 3. PER. = period of coherent pulsation, (transient if followed by t). 4. PER. = second period of coherent pulsation, (transient if followed by t). DQ : 3. PER. = rotation period of the white dwarf. 4. PER. = optical period, (presumably due to reprocessed x-rays). XP : 3. PER. = pulse period of the pulsar. 4. PER. = optical period, (presumably due to reprocessed x-rays). The occurrence of transient quasi-periodic oscill- ations (QPO) in objects of type N, DN, NL, XL, XT, XB and XP is indicated in the field u_P3. s u_P3 "Q" means occurrence of transient quasi-periodic oscillation "T" means transient ":" means unaccurate --- P4 Additional Periods: fourth period s EB indicates the occurrence of eclipses indicates the occurrence of eclipses if blank no eclipses observed if 1 1 eclipse per orbital revolution observed if 2 2 eclipses per orbital revolution observed if d periodic eclipse-like dips observed --- SB Type of spectroscopic binary (1 or 2) type of spectroscopic binary if 1 single-lined spectroscopic binary if 2 double-lined spectroscopic binary --- TClass Temperature class The number indicates the luminosity class , i.e. I = 1 II = 2 III = 3 IV = 4 V = 5 --- LClass Luminosity class (4=IV or 5=V) --- u_LClass uncertain value when ":" --- Sp_1 Spectral type of the primary --- M1/M2 Mass ratio M1/M2 --- u_M1/M2 may be uncertain ":" --- e_M1/M2 error of M1/M2 --- l_incl limit inclination may be "<" --- incl Orbital inclination (in degrees) deg u_incl uncertain value when ":" --- e_incl error in inclination deg l_M1 limit primary mass may be "<" --- M1 mass primary (in solar masses) solMass u_M1 uncertain M1 value when ":" --- e_M1 error in primary mass solMass M2 Mass of the secondary (in solar masses) solMass u_M2 uncertain value when ":" --- e_M2 error in M2 solMass Catalog of Low-Mass X-Ray Binaries OBJECT Object name --- Alt Alternative name --- RAh Right Ascension J2000 hours h RAm RA minutes min RAs RA seconds s DE- Sign Declination J2000 --- DEd Declination J2000 Degrees deg DEm Declination arc minutes arcmin DEs Declinations arc seconds arcsec CoordAcc Accuracy of the coordinates, in hexadecimal number (A=10") --- OType1 first object type characterization --- u_OType1 may be a "?" --- OType2 second object type characterization --- u_OType2 may be a "?" --- OType3 third object type characterization --- l_mag1 limit on mag1 may be ">" or "<" --- mag1 magnitude mag n_mag1 a "B" means that the magnitude is blue (visual otherwise) --- l_mag2 limit on mag2 may be ">" --- mag2 magnitude --- n_mag2 a "B" means that the magnitude is blue (visual otherwise) --- mag3 magnitude mag LX/LO X-ray to optical luminosity ratio --- T1 Typical time interval between outbursts (in days) or minimum value d PerOrb Orbital period, in days d n_PerOrb a ":" means uncertain value --- P2 Second period, in days d P3 Additional periods: third period s u_P3 "Q" means occurrence of transient quasi-periodic oscillations --- P4 Additional Periods: fourth period s EB indicates the occurrence of eclipses --- SB Type of spectroscopic binary (1 or 2) --- Sp_1 Spectral Type of the primary --- LClass Luminosity class (4=IV or 5=V) --- u_LClass uncertain value when ":" --- M1/M2 Mass ratio M1/M2 --- u_M1/M2 may be uncertain ":" --- e_M1/M2 error of M1/M2 --- l_incl limit inclination may be "<" --- incl Orbital inclination (in degrees) deg u_incl uncertain value when ":" --- e_incl error in inclination deg l_M1 limit primary mass may be "<" --- M1 mass primary (in solar masses) solMass u_M1 uncertain M1 value when ":" --- e_M1 error in primary mass solMass M2 Mass of the secondary (in solar masses) solMass u_M2 uncertain value when ":" --- e_M2 error in M2 solMass Catalog of Related Objects OBJECT Object name --- Alt Alternative name --- RAh Right Ascension J2000 hours h RAm RA minutes min RAs RA seconds s DE- Sign Declination J2000 --- DEd Declination J2000 Degrees deg DEm Declination arc minutes arcmin DEs Declinations arc seconds arcsec CoordAcc Accuracy of the coordinates, in hexadecimal number (A=10") --- OType1 first object type characterization --- OType2 second object type characterization --- mag1 magnitude mag n_mag1 a "B" means that the magnitude is blue (visual otherwise) --- l_mag2 limit on mag2 may be ">" --- mag2 magnitude --- n_mag2 a "B" means that the magnitude is blue (visual otherwise); the colon indicates an uncertain value. --- PerOrb Orbital period, in days d n_PerOrb a ":" means uncertain value --- P2 Second period, in days d EB indicates the occurrence of eclipses --- SB Type of spectroscopic binary (1 or 2) --- Sp_1 Spectral Type of the primary --- LClass Luminosity Class (4=IV or 5=V) --- Sp_2 Spectral Type of the secondary --- l_ecc limit on the eccentricity ecc --- ecc eccentricity of the orbit --- e_ecc error in the eccentricity --- M1/M2 Mass ratio M1/M2 --- u_M1/M2 may be uncertain ":" --- e_M1/M2 error of M1/M2 --- l_incl limits on the inclination --- incl Orbital inclination (in degrees) deg e_incl error in inclination deg M1 mass primary (in solar masses) solMass u_M1 uncertain M1 value when ":" --- e_M1 error in primary mass solMass l_R1 limit on radius of primary --- R1 radius primary solRad e_R1 error in radius primary solRad M2 Mass of the secondary (in solar masses) solMass u_M2 uncertain value when ":" --- e_M2 error in M2 solMass R2 radius secondary solRad u_R2 uncertain value radius secondary --- e_R2 error in radius secondary solRad Object Listing by Lexigraphical Name Object listing by right ascension OBJECT Object name --- n_OBJECT Alias present when * --- RAh Right Ascension J2000 h RAm RA minutes min RAs RA seconds s TS Page number Catalog Table in catalog.doc --- RS Page number Reference in catalog.doc --- FC Page number finding chart in catalog.doc --- references to data from cataclysmic variables references to data from Low Mass X-Ray Bin. references to data from related objects references to finding charts Ref Reference Code --- RefNo Reference Number --- RefText Reference Text --- catalog.doc *Complete documentation in print format of the catalog for Cataclysmic binaries, LMXRB, and the related objects. The first character is for Fortran carriage control ('0' is linefeed, '1' is formfeed). In order to obtain a proper printout the length of the forms should allow for up to 64 lines per page and the width sufficient to print 128 columns. Page numbers are given in columns 128-129. The errors listed in the "note added in proof" of the original paper were corrected. * The file can easily be transformed into a printable file on a Unix station with the shell command: awk 'BEGIN{c[0]="\n";c[1]="\f"}{print c[substr($0,1,1)] substr($0,2)}' print Francois Ochsenbein CDS Paul Kuin ADC/NASA 1995 Oct 25 The author is grateful to all the colleagues who have contributed by sending pre- and reprints of relevant papers. This work was supported in part by the Deutsche Forschungsgemeinschaft, grant KU 474/13-2. UNKNOWN UNKNOWN Original received from Dr. Ritter by CDS. NASA ADC converted the documentation to standard format in June 1995. The original catalogue contained 3 files: the format documentation, the catalog in print-out format and the documentation. The format documentation was reformatted and absorbed in this ReadMe file. Information from the full catalog documentation was also used to complete the ReadMe file. Tables were extracted for the low-mass X-ray binaries and related objects and reformatted. CDS added the notes about printing the print file and generated some changes to the labels and text. The contributions of ADC and CDS were combined. UNKNOWN UNKNOWN the printed version of the catalog: The file catalog.doc is the catalogue in print-out format. 4409 records of 132 bytes. The first character is for carriage control. In order to obtain a proper printout the length of the forms should allow for up to 64 lines per page and the width sufficient to print 128 columns. Page numbers are given in columns 128-129. The errors listed in the "note added in proof" of the original paper were corrected. The content of the complete catalog including full documentation is contained in this file. It includes a list of objects in lexigraphical order and in order by right ascension, a description of the table headings and abbreviations, the table and reference sections of the catalog, the references for the finding charts, and a list of aliases for the objects. Parts of this file have been extracted into the other data files. For the current version of this catalogue, literature published before December 31, 1989 has, as far as possible, been taken into account. V_59.xml The Almagest: Ptolemy's star catalogue (years 127-141) 5061 V/61 Almagest The Almagest: Ptolemy's star catalogue (years 127-141) C Ptolemy translation by Manitius K.,ed. B.G. Teubner, Leipzig ??? ??? 1913 1987BICDS..33..125J The Almagest: Ptolemy's star catalogue (years 127-141) C Jaschek Bull. Inform. CDS 33 125 1987 1987BICDS..33..125J V/50 : (The Bright Star Catalogue) Historical catalog This catalogue is the machine readable version of the star catalogue given by Claudius Ptolemy in his book called usually the Almagest. It is based upon its translation by K. Manitius (ed. B.G. Teubner, Leipzig 1913). The table reproduces the values given in book VII, chapter V, namely Identification, name, longitude, latitude and magnitude. To facilitate its use the following changes were made: Identifications : the numbers of Ambronn's catalogue (used by Manitius) were replaced by the numbers in the Bright Star Catalogue (D. Hoffleit and C. Jaschek - Fourth edition - Yale University Observatory 1982) which are commonly used today. Name : we have kept the Bayer names but omitted the description given by Manitius (for instance alpha UMi = that of the end of the tail). Whenever a disagreement exists concerning the identification of a given star, this is signaled by a "D" (disagreement) in the notes (last column). The list of disagreements was taken from Werner H. and Schmeidler F., "Synopsis der Nomenklatur der Fixsterne" - Wissensch. Verlags-Gesellschaft Stuttgart (1986) where the interested reader may find detailed references. Most of the disagreements stem from the work of Peters and Knobel, Washington 1915. Longitude : the Ptolomean longitudes were converted into the commonly used longitudes by adding 0 to longitudes in Aries, 30 to those in Taurus, etc. Longitudes vary thus between 0 and 360 . Latitudes : no change from Ptolemy. Magnitudes : no change from Ptolemy. Notes : "D" stands for disagreements over identifications, see above. With the publication of a computer readable version of this catalogue we hope to satisfy a long standing need. We also pay in this way our debt of gratitude toward the astronomer who produced the most used catalogue in the history of astronomy - for more than fourteen centuries it was THE catalogue by definition. It seems only appropriate that a data center, who is in a long way a descendant of such an enterprise, includes the catalogue in its collection.
Northern part (except Zodiacal stars) Southern part (except Zodiacal stars) Zodiacal stars, North Zodiacal stars, South Const Constellation name --- HR Bright Star Number, 0 if cluster --- m_HR Second HR number for binaries --- Seq Number in constellation --- Lon.d Ptolemean (ecliptic) longitude (degrees) number=1 the Ptolomean longitudes were converted by adding 30deg in Taurus etc (see Description). The epoch of observation is compared to -128 by Grasshoff G., 1990, "The history of Ptolemy's Star Catalogue", ed. G.J. Toomer, Springer-Verlag (ISBN 0-387-97181-5) deg Lon.m Ptolemean (ecliptic) longitude (minutes) number=1 the Ptolomean longitudes were converted by adding 30deg in Taurus etc (see Description). The epoch of observation is compared to -128 by Grasshoff G., 1990, "The history of Ptolemy's Star Catalogue", ed. G.J. Toomer, Springer-Verlag (ISBN 0-387-97181-5) arcmin Lat- Ptolemean (ecliptic) latitude (sign) --- Lat.d Ptolemean (ecliptic) latitude (degrees) deg Lat.m Ptolemean (ecliptic) latitude (minutes) arcmin Mag Ptolemean magnitude number=2 the Ptolomean magnitudes are only integer numbers between 1 and 6; the values "7." correspond to "faint", and "8." for "nebula". The decimal value "m.3" (m between 1 and 4) indicate original "(m)-(m+1)" The decimal value "m.7" (m between 1 and 4) indicate original "(m-1)-(m)" Examples: "2.7" correspond to original "3-2" "3.3" correspond to original "3-4" mag Disag 'D' if a disagreement exists concerning identification --- Francois Ochsenbein CDS 1995 Jul 17 UNKNOWN UNKNOWN * 1987: Keypunched at CDS, Strasbourg; original technical note prepared by O.Yu. Malkov * 17-Jul-1995: Documentation standardized at CDS V_61.xml Eighth catalogue of the orbital elements of spectroscopic binary systems. 5064 V/64 Eighth Orbital Elements of Spectroscopic Binaries Eighth catalogue of the orbital elements of spectroscopic binary systems. A H Batten J M Flechter D G MacCarthy Publ. Dominion Astrophys. Obs. 17 ??? ??? 1989 1989PDAO...17....1B V/41 : Physical parameters of SBs (Kraicheva+ 1980) Batten A.H., Flechter J.M., Mann P.J., 1978, "7th Catalogue of the orbital elements of spectroscopic binaries", Publ. Dom. Astrophys. Obs. 15, 121 (catalogue <V/40>) Binaries, orbits Binaries, spectroscopic The complete description of the catalogue, as well as the notes, is to be found in the Publ. Dominion Astrophys. Obs. 17 (1989). The present machine-readable version was transformed from the file provided by A.H. Batten for easier computer readability. Compared to the printed version, please note the following: 1) The four columns No. f(m) m.sin^3(i) a.sin(i) are NOT included in the computer version. No. (running number) is the line number of the main file (from 1 to 1469) f(m) (expressed in Solar Masses) can be computed from the Fortran formula 1.0385E-7 * (1-e*e)**1.5 * K(1)**3 * P a(*)sin i (expressed in km) can be computed from the Fortran formula 13751 * sqrt(1-e*e) * K(*) * P m(*)sin3i (expressed in Solar Masses) can be computed from the Fortran formula 1.0385E-7 * (1-e*e)**1.5 * K(*) * (K(1)+K(2))**2 * P The parameters are K(*) = velocity amplitude of the components, expressed in km/s; P = Period, expressed in days, sometimes in years; e = eccentricity 2) The notes, which make the bulk of the printed catalogue (pages 129-304), are NOT included.
The 8th catalogue of orbital elements of SBs RAh RA 1900 (hours) h RAdm RA 1900 (deci-minutes) dmin DE- DEC1900 (sign) --- DEd DEC1900 (degrees) deg DEm DEC1900 (arcminutes) arcmin --- Separation character --- Name First name. Just a number means HD number number=1 note that greek letters and other symbols use TeX conventions --- --- Separation character --- Alias Other Name number=1 note that greek letters and other symbols use TeX conventions --- Eclipse The '*' indicates an eclipsing binary --- --- Separation character --- maxMag Magnitude at Maximum mag n_maxMag Type of maxMag magnitude number=2 B, V or R indicate a photoelectric magnitudes; P indicates a Photographic magnitude --- f_maxMag Remark or Note flag --- --- Separation character --- minMag Magnitude at Minimum mag n_minMag Type of minMag magnitude number=2 B, V or R indicate a photoelectric magnitudes; P indicates a Photographic magnitude --- f_minMag Remark or Note flag --- --- Separation character --- Sp1 Spectral type of Primary --- --- Separation character --- Sp2 Spectral type of Secondary (if known) --- --- Separation character --- Period Period, generally in days (see x_Period) --- x_Period 'y' if Period expressed in years --- f_Period Remark or Note flag --- --- Separation character --- T Periastron date, generally in JD-2400000 (see x_T indicator) --- x_T 'y' if periastron T expressed as year. --- f_T Remark or Note flag --- --- Separation character --- e1 Eccentricity of Primary --- f_e1 Remark or Note flag --- --- Separation character --- e2 Eccentricity of Secondary, if different --- --- Separation character --- omega1 Angle of periastron of Primary deg u_omega1 Uncertainty flag (:) --- f_omega1 Remark or Note flag --- --- Separation character --- omega2 Angle of periastron of Secondary deg u_omega2 Uncertainty flag (:) --- f_omega2 Remark or Note flag --- --- Separation character --- K(1) Orbital semi-amplitude of Primary km/s u_K(1) Uncertainty flag (:) --- f_K(1) Remark or Note flag --- --- Separation character --- K(2) Orbital semi-amplitude of Secondary km/s u_K(2) Uncertainty flag (:) --- f_K(2) Remark or Note flag --- --- Separation character --- V(1) Systemic Velocity of Primary km/s u_V(1) Uncertainty flag (:) --- f_V(1) Remark or Note flag --- --- Separation character --- V(2) Systemic Velocity of Secondary km/s u_V(2) Uncertainty flag (:) --- f_V(2) Remark or Note flag --- --- Separation character --- f_Quality Remark or Note flag --- Quality Quality letter number=3 the Quality letter has the following meaning: a = Definitive orbit b = Good orbit, but not definitive c = Average orbit d = Poor orbit e = Very poor and unreliable orbit i = insufficient information --- --- Separation character --- Ref Reference (makes use of TeX conventions) --- Francois Ochsenbein CDS 1997 Oct 20 UNKNOWN UNKNOWN * June 1991: the catalogue was copied from ftp anonymous at dao.nrc.ca * January 1992: catalogue transformation and first documentation made by Francois Ochsenbein, Centre de Donnees Astronomiques, Strasbourg (France), * 16-Apr-1996: Documentation standardized at CDS. The position of entry #874 (2S1553-42) was corrected . The declination of entry #1057 (HD 170000) was corrected. * 20-Oct-1997: Thanks to a remark by Steve Drake <drake@lheavx.gsfc.nasa.gov>, the spectral types of secondary (Sp2) which were missing have been added. V_64.xml A Spectroscopically Selected Catalog of K Giants in the Galactic Halo 5065 V/65 Spectroscopically Selected Gal Halo K Giants A Spectroscopically Selected Catalog of K Giants in the Galactic Halo K U Ratnatunga K C Freeman ApJ 339 126 1989 1989ApJ...339..126R Abundances, [Fe/H] Radial velocities Stars, giant Stars, halo Stars, high-velocity The catalog results from a survey for distant Field K giants in the Galactic halo made for purposes of locating a chemically and kinematically unbiased sample out to about 25 kpc from the Sun. The motivation for the study and sample selection are outlined by Ratnatunga & Freeman (1985), while details and analysis of the results will be found in Ratnatunga & Freeman (1989). Three high-galactic-latitude fields each of 20 square degrees, designated by their Selected-Area identifications, include the following: SA 141 (l=240,b=-85); SA 189 (277, -50); and SA 127 (272, +38), and have the apparent magnitude range 13 < V < 16 and color range (B-V) > 0.9. Stars were selected from PDS photographic photometry of Schmidt plates (see Ratnatunga 1983, catalog #2121). K-giant selection used the Mgb+MgH feature at 5100A from digital image analysis of PDS scans of ESO 1-m Schmidt telescope objective-prism spectra with 450 A/mm at H-gamma resolution on IIIa-J plates exposed through a Schott GG475 filter. Luminosity confirmation, line-of-sight velocities, and metallicity were determined from 2-A resolution slit spectra taken with the 4-m Anglo- Australian and 1.9-m Mount Stromlo telescopes. Cross identifications exist for some stars in the SA 141 SGP field only.
Catalog Data GLON Galactic longitude deg GLAT Galactic latitude deg V Photoelectric V magnitude on UBV system mag B-V Photoelectric B-V color on UBV system mag M(V) Absolute visual magnitude mag [Fe/H] Fe/H value relative to Sun (brackets omitted) --- D Photometric distance kpc RV Radial (line-of-sight) velocity km/s RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAds Right Ascension 1950 (deci-seconds) 0.1s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RF Star designation from Ratnatunga (1983) --- E Star designation from Eriksson (1978) --- BB Star designation from Bok & Basinski (1964) --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Aug 16 UNKNOWN UNKNOWN The catalogue was received from the Astronomical Data Center; the Format part has been standardised at CDS. Original summary and format description was prepared at the Astronomical Data Center, National Space Science Data Center / World Data Center A for Rockets and Satellites, NASA Goddard Space Flight Center. Wayne H. Warren Jr., Kavan U. Ratnatunga, 1990 November. V_65.xml A Catalog of Observations for Stellar Masers 5068A V/68A Stellar Maser Observations A Catalog of Observations for Stellar Masers P J Benson I R Little-Marenin J Attridge K Blais D Randolph T Woods M Rubiera H Keefe ApJS 74 911 1990 1990ApJS...74..911B Masers Stars, masers This catalog contains about 2958 stellar sources. For the searching of the maser emission of the sources listed, 368 were detected in H2O, 209 in SiO, and 713 in OH. In the catalog, one can find information about the stars including alternate names, the 1950 epoch position, velocity (LSR), spectral type, variability type, and period, as well as the references for both the detections and nondetections for each of the three molecules. In this catalog, Table 1 lists all the sources in right ascension order, Table 2 lists the references for all the maser observations for each source, and Table 3 lists the references in code order, i.e., in chronological order.
Basic stellar data ObsNum Number in Right Ascension order The number differs from the publication --- Name Generally Variable name (GCVS) (constellation in 21-23) --- Name2 Second name --- Name3 Third name (generally IRAS) --- RAh RA hours (1950) h RAm RA minutes (1950) min RAs RA seconds s DE- Dec sign --- DEd Dec degrees (1950) deg DEm Dec arcminutes arcmin DEs dec arcseconds arcsec VLSR LSR radial velocity; km/s u_VLSR asterisk means heliocentric velocity --- SpType Spectral type --- VarType Variable type --- Period Period in days d u_Period Uncertainty flag (:) on Period --- H2O detected in H2O? The field for detected H2O, SiO, or OH is blank if no observations was published. --- SiO detected in SiO? --- OH detected in OH? --- note Comments --- Bibliography and comments ObsNum Number as in table1 --- Name Name as in table1 --- Mol Molecule H2O, SiO or OH --- RefID Reference detailed in file refs --- Note Result of observation N indicates that the observation was negative; T indicates a thermal emission of SiO * = N T ? indicates an uncertain detection . when there is a comment --- Comment Text of comment --- References RefID Reference code, as in table2.dat --- Author1 author1 --- Author2 author2 --- Author3 author3 --- Author4 author4 --- Author5 author5 --- Author6 author6 --- Author7 author7 --- Author8 author8 --- Author9 author9 --- Author10 author10 --- Title title --- Journal journal --- Volume volume --- Page page --- Btitle book-title --- Editor1 editor1 --- Editor2 editor2 --- Pub publisher --- City city --- C.-H. Joseph Lyu Hughes STX/NASA Francois Ochsenbein CDS 1997 Oct 16 Priscilla Benson <PBENSON@WELLESLEY.EDU> UNKNOWN UNKNOWN 16-Mar-1992: first version at CDS 16-Aug-1995: Modifications by C.-H. Joseph Lyu [Hughes STX/NASA] 16-Oct-1997: Reformatted by F. Ochsenbein [CDS] UNKNOWN UNKNOWN For the 2958 stellar sources listed in this catalog, 1769 had been searched for H2O emission. and it was detected in 368 (21%) of those observed; 639 sources had been searched for SiO emission with detections in 209 (33%); and 2253 sources had been searched for OH emission with detections in 713 (32%). Because strong biases found in the data the percentages should be interpreted with caution. For detailed bias information, please consult Benson et al. (1990). V_68A.xml Third Catalog of Emission-Line Stars of the Orion Population 5073A V/73A Third Cat Em-Line Stars of the Orion Population Third Catalog of Emission-Line Stars of the Orion Population G H Herbig K R Bell Lick Observatory Bull. No. 1111 ??? ??? 1988 1988LicOB1111....1H Combined data stars, pre-main sequence This Catalog lists 735 pre-main sequence stars, members of the Orion Population, that have been observed with slit spectrographs or at equivalent resolution. It is intended to replace the Second Catalog of Herbig and Rao (1972). It gives accurate coordinates (many determined especially for this Catalog), light ranges for known variables, UBVRI data near maximum light, references to ultraviolet, X-ray and radio observations and to light curves, value of v sin i and the radial velocity when known, spectral type, equivalent width of the H-aplha emission line, references to spectral reproductions or scans and spectroscopic studies and to identification charts, and a classification (as a T Tau star, FU Ori object, etc.)
This is the third up-date of a listing of the pre-main sequence stars, both certain and probable, that have emission lines and that have been observed with slit spectrographs or at comparable resolution. The first (Herbig 1962) contained 126 entries, the second (Herbig and Rao 1972: hereafter HRC) had 323, while the present Catalog contains 735. Not only has the total number of stars increased due to a higher level of observational activity and the improvement of spectroscopic instrumentation, but there is a greater variety of significant information to be referenced: for example, there was no occasion in earlier listings to mention v sin i's, radial velocities, far-ultraviolet, X-ray or radio-frequency data. The classification scheme for pre-main sequence stars (described below) has also been modified as the result of improved observational information. In order to accommodate such new information as well as more accurate astrometric coordinates within a double page, 264-column format, it has been necessary to omit some information that is relevant and would have been useful in some cases: (a) IRAS identifications are not included. (b) Light curve classifications are not included, partly because such traditional observations have not kept pace with the volume of other information. Instead, references are given to sources where such information as exists may be found, except in cases where rotational modulation has been detected; such results are given in the Remarks to Table 1. (c) No references are given to polarization information; however, that subject has recently been surveyed very thoroughly by Bastien (1988). (d) The "emission line intensity" classification of the Second Catalog, a rather subjective quantity but all that was available in 1972, has been replaced by the equivalent width of H-alpha emission, which is now readily determinable as the result of the widespread use of linear, red-sensitive detectors. (e) No references are given to proper motion information. The numbers assigned by Herbig and Rao (1972), prefixed HRC in the past, have been retained for those of the 323 stars of the Second Catalog that have survived subsequent examination. Thus the new entries begin with 324 and extend through 742. The ordering is strictly in order of right ascension for 1950.0. As the result of improved coordinates, the original HRC ordering is sometimes altered. It is suggested that Catalog entries be referred to by their primary designation, which usually is in the 'name' column. In circumstances where the Catalog number must be used, it is recommended that HRC now be replaced by HBC. Note also that the letter n or an asterisk (*) which often follow the HBC number are not part of that designation, but are separate items of information. It was suggested in the Second Catalog that many of the variables in young clusters and associations that were not then known to have line emission would turn out to have bright H-alpha or Ca II, H,K lines upon closer examination. This has turned out to be so: many such stars are now included as "weak-line T Tauris" (abbreviation: wt). A large number of such stars have also been recognized as the result of X-ray surveys of obscured regions, particularly the Taurus-Auriga clouds. Walter and co-workers, who have done much of this work, have called these objects "naked T Tauri stars", or NTTS. It is our opinion that these do not constitute a separate class of pre-main sequence stars, but are a quite natural extension of the T Tauri class toward weaker line emission since the cutoff of conventional T Tauri stars at W(H-alpha) ~ 5 A was set only by the limitations of the early objective-prism or -grating surveys. The existence of substantial numbers of such stars was in fact to be expected (Herbig 1985) from the shape of the frequency distribution of W(H-alpha). We prefer the non-committal classification "wt" for these stars as a group rather than NTTS, partly because the latter implies a physical picture of the phenomenon that is still speculative. However, one kind of weak-emission star that has been omitted from the Third Catalog are the rapid-rotating G- and K-type dwarfs in young clusters, such as alpha Per and the Pleiades, most of which have emission at H-alpha. They have not been included because they lie on or near the main sequence. There are probably such stars in the field as well, and consequently we have omitted objects such as W92/NGC 2264 (= V642 Mon), Gliese 182 (= V1005 Ori), and any others that appear to be BY Dra-like variables. On the other hand, we have included many weak-emission G and K stars in the Orion Nebula region and in NGC 2264, on the grounds that they lie well above the main sequence and are therefore clearly pre-main sequence objects. The lower boundary of the Orion population, insofar as it is represented in this Catalog, thus is not well defined. Nor is it always apparent whether a late-type star having no more than weak H-alpha and Ca II emission is pre-main sequence or not. This is a relatively recent problem. The sample of emission objects that were turned up in the early H-alpha surveys were mostly classical T Tauri stars, where emission-line criteria clearly provide the identification. Foreground dMe stars were not detected, because such stars in the field and in older aggregates like the Hyades rarely have W(H-alpha) greater than about 6 A. But in younger clusters like the Pleiades, emission H-alpha has now been found in M dwarfs at W(H-alpha) values as large as 18 A, although the most are less than 12 A (Stauffer and Hartmann 1986). When such stars attract scrutiny as the consequence of some special activity, such as variability or X-ray emission, unless their luminosity is well enough known to locate them above the main sequence, there is no obvious way to distinguish a pre-main sequence star from its young main sequence counterpart. It is possible that refinement of the lithium abundance criterion might clarify this situation. It must be stressed that the stars listed here have been discovered by a variety of techniques, through searches that have been concentrated in certain areas while other regions have been almost neglected. Therefore, no one should consider the Catalog as complete even to a fairly modest limiting magnitude over any large fraction of the sky. The Catalog references those sources and papers that were available to us through March 1988. We shall be grateful for any errors that are called to our attention. The Catalog: Catalog.dat contains both real data as well as references to published papers, the latter have been listed in refs.dat. In the following text, the numbers assigned to papers in the Reference list are in [square brackets]. Within that list, for journals which exist both in the original language and in English translation, the English-language citation is given first, followed by the original in brackets (thus: Sov.Astr.-A.J. 7, 219 [7, 398]).
Catalog Data HBC HBC number. The running number is followed by n when the star itself is involved in, or illuminates bright nebulosity. An asterisk (*) indicates that a Remark follows the Table. --- nebu_flg Nebulosity association flag. --- rem Remark flag. See file remarks.dat --- name Star name. This is the preferred designation of the object; if a variable star name has been assigned that is always given preference. If the preferred name is too long, a > symbol indicates that it follows in col. 3. --- alt Other designation. Other designation: The conventional designations (AS, LkHalpha, Haro ...) are explained in HRC. We have found it necessary in some cases to expand the prefix system, usually abbreviating discoverers' names by two-letter symbols rather than one to avoid confusion with variable star designations (thus: CoKu for Cohen and Kuhi). We have also retained the discoverer's name for an object wherever possible, rather than substituting what might seem a more rational designation (thus: P2441/c for the companion of P2441, rather than P2441 B). The prefixes used in cols. 2, 3 are as follows: CD Cape Photographic Durchmusterung CoD Cordoba Durchmusterung CoKu Cohen and Kuhi [93] Eggen [125] Elias Tau-Aur [128]; Oph [127]; IC 5146 [126] FK Feigelson and Kriss [132] GlPe Glass and Penston [157] GM Gyulbudaghian and Magakyan [177] HaGr Hartigan and Graham [186] He 3- Henize [195] HH Herbig [211] and later publications by a variety of authors. HJ Herbig and Jones [218] HJM Hyland, Jones and Mitchell [238] HM Henize and Mendoza [196] JH Jones and Herbig [250] Kn Knacke et al. [274] LkCa Herbig, Vrba and Rydgren [219] LZK Liu, Zhang and Kimura [315] MacC MacConnell 1968: Cep-Cas; 1981: Pup MaRy Marraco and Rydgren [323] MC Cohen [90] NTTS Walter et al. [506] OgHa Ogura and Hasegawa [355] P 4 digits: Parenago [359] 1 digit: Mundt et al. [344] Par Parsamian [360] PC Parsamian and Chavira [363]: PC numbers have been assigned to all the confirmed Tonantzintla discoveries in the Orion Nebula region, but Table 1 gives only those that have no Haro 6- designations. PH Pettersson [370, 371] PP Parsamian and Petrossian [362] ROX Montmerle et al [332] RNO Cohen [85] S Sonneberg variable star San Sanduleak [417] SS 1 Sanduleak and Stephenson [419a] SS 2 Stephenson and Sanduleak [444a] SSS Strom, Strom and Stocke [450] SSV Strom, Vrba and Strom [455] St Stephenson [444] Sz Schwartz [426] TH The: see Table 3 vBH van den Bergh and Herbst [482] VSB Vasilevskis, Sanders and Balz [485] W Walker, NGC 2264 [494]; IC 5146 [495] Wa Walter [502] WK Walter and Kuhi [504] Wray Wackerling 1970 --- RAh Hours of right ascension (1950.0). The coordinates indicated by B in col. 6 were determined by one of us (KRB) with the Lick Automatic Measuring Machine on yellow (in most cases) plates of the Lick astrometric program. Usually 15 to 20 reference stars from the AGK3, with proper motions applied, were used. The epoch (minus 1900), rounded off to the nearest year, follows the B. The coordinates indicated by Aw in col. 6 were originally measured by C.A. Wirtanen, from blue plates of the Lick program, for the HRC. The epoch of those coordinates is approximately 1950. We do not regard either B or Aw coordinates to be of astrometric quality. Coordinates drawn from other sources are referenced accordingly. Those brought forward to 1950.0 have not had proper motions applied, so remain at their original epoch. h RAm Minutes of right ascension. The coordinates indicated by B in col. 6 were determined by one of us (KRB) with the Lick Automatic Measuring Machine on yellow (in most cases) plates of the Lick astrometric program. Usually 15 to 20 reference stars from the AGK3, with proper motions applied, were used. The epoch (minus 1900), rounded off to the nearest year, follows the B. The coordinates indicated by Aw in col. 6 were originally measured by C.A. Wirtanen, from blue plates of the Lick program, for the HRC. The epoch of those coordinates is approximately 1950. We do not regard either B or Aw coordinates to be of astrometric quality. Coordinates drawn from other sources are referenced accordingly. Those brought forward to 1950.0 have not had proper motions applied, so remain at their original epoch. min RAs Seconds of right ascension. The coordinates indicated by B in col. 6 were determined by one of us (KRB) with the Lick Automatic Measuring Machine on yellow (in most cases) plates of the Lick astrometric program. Usually 15 to 20 reference stars from the AGK3, with proper motions applied, were used. The epoch (minus 1900), rounded off to the nearest year, follows the B. The coordinates indicated by Aw in col. 6 were originally measured by C.A. Wirtanen, from blue plates of the Lick program, for the HRC. The epoch of those coordinates is approximately 1950. We do not regard either B or Aw coordinates to be of astrometric quality. Coordinates drawn from other sources are referenced accordingly. Those brought forward to 1950.0 have not had proper motions applied, so remain at their original epoch. s DE- Sign of declination (1950.0). --- DEd Degrees of declination. deg DEm Minutes of declination. arcmin DEs Seconds of declination. arcsec u_RAh Position uncertainty flag (:) The coordinates indicated by B in col. 6 were determined by one of us (KRB) with the Lick Automatic Measuring Machine on yellow (in most cases) plates of the Lick astrometric program. Usually 15 to 20 reference stars from the AGK3, with proper motions applied, were used. The epoch (minus 1900), rounded off to the nearest year, follows the B. The coordinates indicated by Aw in col. 6 were originally measured by C.A. Wirtanen, from blue plates of the Lick program, for the HRC. The epoch of those coordinates is approximately 1950. We do not regard either B or Aw coordinates to be of astrometric quality. Coordinates drawn from other sources are referenced accordingly. Those brought forward to 1950.0 have not had proper motions applied, so remain at their original epoch. --- r_RAh References to the position. The coordinates indicated by B in col. 6 were determined by one of us (KRB) with the Lick Automatic Measuring Machine on yellow (in most cases) plates of the Lick astrometric program. Usually 15 to 20 reference stars from the AGK3, with proper motions applied, were used. The epoch (minus 1900), rounded off to the nearest year, follows the B. The coordinates indicated by Aw in col. 6 were originally measured by C.A. Wirtanen, from blue plates of the Lick program, for the HRC. The epoch of those coordinates is approximately 1950. We do not regard either B or Aw coordinates to be of astrometric quality. Coordinates drawn from other sources are referenced accordingly. Those brought forward to 1950.0 have not had proper motions applied, so remain at their original epoch. --- GLON Galactic longitude. Galactic coordinates in the lII, bII system deg GLAT Galactic latitude. deg phot_range Photometric range. Photometric range if the star is a known variable, expressed in the magnitude system indicated. Values taken from the 4th edition (1985, 1987) of the General Catalogue of Variable Stars, or recent Supplements, are indicated by a C. (Note that the conventional practice is followed in that < means "fainter than".) Stars believed to be variable are indicated var. A number of stars not known to be variable have their mean, or estimated magnitudes in these columns if that magnitude is not visual or in the Johnson V system; otherwise that value is in the "V" column. --- mag_sys Code to the magnitude system. --- phot_ref Photometric references. --- l_V Inequality sign to the V magnitude. --- V V magnitude. V, B-V, U-B photometry: for stars observed more than once, unlike HRC practice (where mean values were given regardless of phase) these columns contain the values observed when the star was brightest in V and a full set of UBVRI magnitudes were measured at essentially the same time. In some cases, the colors show a substantial scatter at the same value of V; such colors are marked with a v. For those stars where there is only a small scatter about a mean V, or where a small-range cyclic variation is superposed upon irregular activity, mean rather than maximum-V values are tabulated; such stars have an m following their V magnitude. mag Vcode Code to the V magnitude. --- B-V B-V color. mag B-Vcode Code to the B-V color. --- U-B U-B color. mag U-Bcode Code to the U-B color. --- refs_UBV References to the UBV data. Photometric references: the first number is the source from which the tabulated values are taken. Additional sources of UBV data follow. For stars having an extensive photometric history, a * means that details are in a Remark to Table 1. An hrc means that some information given in the Second Catalog is not repeated here. --- V-R V-R color. V-R, V-I values, usually obtained simultaneously (i.e., at maximum V) with the UBV data of cols. V, B-V, U-B; this is so if the first reference in col. refs_VRI is the same as the first in col. refs_UBV. mag V-Rcode Code to the V-R color. --- V-I V-I color. mag V-Icode Code to the V-I color. --- RI_code Code to the (R,I) system. A single letter (J, C) shows whether the R, I values are on the Johnson or Cousins system. An i indicates an instrumental (r,i) system; conversion relations for the photometry by Rydgren and co-workers are given in [407]. --- refs_VRI References to the VRI data References to the V-R, V-I data, as described for col. refs_UBV. --- refs_IR References to the infrared magnitudes. References for infrared magnitudes, spectrophotometry and spectroscopy. However, low angular resolution far-infrared observations are not usually cited. --- refs_UVX X-ray references. UV, X-ray references: these usually refer to IUE spectroscopy and to X-ray detections from the Einstein survey. --- refs_radio Radio references. Radio references are to VLA observations or to detection of the star by some other means. No attempt is made to cite radio frequency molecular line observations of the cloud in the general neighborhood of the star. --- refs_lc References to the light curves. Light curve: references to photometric studies published since HRC. An hrc means that significant references in the Second Catalog are not repeated here. --- l_vsini Inequality sign to the (v sin i). --- vsini (v sin i) data. v sin i, the projected axial rotational velocity, given only to the nearest km/s. If no radial velocity value appears in col. RV, then that reference is to the source of the v sin i; if a value for the radial velocity is given, then the second reference is (usually) the source of the v sin i. km/s vsini_code Code to the (v sin i) data. --- RV Radial velocity. Radial velocity (heliocentric, in km/s), quality, and reference. In all cases, these velocities are from the absorption line spectrum. Velocities obtained with modern equipment usually replace those obtained at low dispersion by the early observers. The quality letter (a, b, c) expresses our judgment as to the uncertainty of the quoted velocity: a indicates a velocity of the highest quality, with an uncertainty of 1-2 km/s; b means a value with an uncertainty of 3-5 km/s; and c a velocity of still lower accuracy. For some stars we have not given the published velocities at all. Comments on several special objects (*) appear in the Remarks. km/s q_RV Quality code to the radial velocity. --- r_RV References to the radial velocity and (v sin i). --- Sp Spectral type. Spectral type. With the growing employment of red-sensitive detectors, spectral types determined since the HRC have increasingly been dependent upon criteria in the region longward of about 5000 A. However, it is apparent that significant differences exist in T Tauri spectra between such types and those assigned by the early observers of the 4000-4500 A region ([498] and Appenzeller 1985). Furthermore, it is not clear whether the spectral types of such stars change during their light variations or at other times. Therefore, it may not be possible to assign a MK type to a T Tauri star without further qualification. We have not faced up to such issues: the types given here for those stars for which more than a single classification is available are either compromise values (usually indicated by :), or in case of conflict that value which seems most reasonable to us. No indication is given of the spectral region in which the type was assigned. Several special cases are explained in the Remarks. Many of the types in HRC were based on unwidened, very low-dispersion, often underexposed Lick spectrograms; in all but a very few cases, those classifications have here been disregarded. The conventions in col. Sp are as in HRC: type K7, M0 means either K7 or M0, while K7-M0 means a type between K7 and M0. If the Li I 6707 A line has been detected in absorption, the type is followed by (Li). The very fact that the star is included in this Catalog indicates that emission lines have been detected (except in a very few special cases, all explained in the Remarks), so the suffix e for emission is not printed for types G and later in col. Sp although it properly is a part of the classification; the e should be added if these types are quoted. However, in order to avoid possible misunderstanding, that e has been included for all the B, A and F types where line emission is present. An hrc means that some significant information either in the Second Catalog, or referenced there, is not repeated. --- r_Sp References to the spectral type. References to the source of the type quoted. Information in col. Sp which does not appear in the papers cited is usually from unpublished Lick material; a blank reference has that specific meaning. --- EW Equivalent width of H-alpha emission. Equivalent width of H-alpha emission (in A): These are from the original sources, and are often mean values. Different observers at different times sometimes quote very different results and it is often uncertain whether this represents real variation or is an instrumental effect; when real variations seem to be present, the mean is given followed by a v. A number of cases where the W(H-alpha) value from slit spectroscopy seems incompatible with the fact of detection of H-alpha on an objective-prism plate are mentioned in the Remarks. A hk in col. EW means that there is no information on H-alpha, but that emission is present in the H,K lines of Ca II. A pr means that H-alpha emission has been detected, but that no value for the equivalent width is available. An abs means that H-alpha is in absorption. An em means that unspecified emission lines have been observed [238]. A * means that there is a Remark (see remarks.dat) . --- EWcode Code to the equivalent width of H-alpha emission. --- refs_Halpha References to the H-alpha emission. --- refs_spec References to the spectrum data. Spectrum references show where the spectrum is reproduced (either photographically or as a scan), or the spectrum is described or discussed. --- type Type of the object. Type gives our judgment as to which group the star belongs. The abbreviations are: tt T Tauri star wt weak-line T Tauri star, usually having W(H-alpha) less than about 10 A and no other emission in the optical region except Ca II H,K. This includes most of the so-called "Naked T Tauri Stars". su A star like SU Aur: type late F to K, weak emission at H-alpha and Ca II, very broad absorption lines (v sin i > 50 km/s), and relatively high luminosity. ae An Ae or Be star such as those described in [203]. fu A star of the type of FU Ori. ? Type uncertain: the information is adequate, but the object does not fit into any established group; these stars are usually described in more detail in the Remarks. Also, one of the original criteria for membership in the Ae, Be group was that the star illuminate bright nebulosity, but now a number of irregular variables are known which are photometrically and spectroscopically similar but are not nebulous or associated with obvious obscuration (UX Ori, WW Vul, SV Cep, BO Cep, ...). These questionable objects are also marked ? , or in some cases a?, in the Table. -- A blank means that the observational information is inadequate. --- refs_chart References to the identification chart. Reference to an identification chart or photograph. --- location Location in the nebulosity. The name of the bright nebulosity, dark cloud, cluster, association, or other object with which the star is associated or projected upon. A number of southern cloud complexes are designated by the abbreviations used by Schwartz [426]; note that these are not the T-association designations of Kholopov (1959) or the R associations of Herbst (1975). The prefixes used are: B Barnard (1927) FS Feitzinger and Stuwe (1984) Gum the Gum Nebula region L Lynds (1962) Ori the Orion Nebula region Sh Sharpless (1959) --- References code Code number for reference --- reftext text reference --- Remarks HBC object HBC identification --- reftext remark text --- N.P.M. Kuin NASA/SSDOO/ADC 1995 Aug 03 We are greatly indebted to A. Klemola for his help with the astrometric measurements, to B.F. Jones for unpublished coordinates and other assistance, and to many colleagues for preprints and unpublished information. We are also very grateful for partial support by the National Science Foundation, most recently under Grant NSF AST82-03115, for much of the observational work at Lick Observatory that is included here as well as for the preparation of the Catalog itself. UNKNOWN UNKNOWN August 1988 (George Herbig): The only differences between this tape and the original paper version are that a few small errors have been corrected, and literature citations have been provided for several papers that were only in press in June 1988. Note that the stars in Table 1 having second-line entries must have those read out of files epage1a and fpage2a, whether first-line data is being taken from cpage1, dpage2 or from epage1, fpage2. Note also that in neither paper nor tape version of this Catalogue was it possible to insert umlauts or accent marks in authors' names. The person who prepared this tape (G.H.) is hardly an an expert, and does not intend to become one. The formatting can undoubtedly be improved, but the tape is (hopefully) readable. Suggestions for the improvement of any future editions would be welcomed. August 1992 (Shiro Nishimura): Reformatting of the catalogue has been made at the Astronomical Data Analysis Center of the National Astronomical Observatory of Japan. The file, epage1 (the main file for the left page), and the file, fpage2 (the main file for the right page), were concatenated with entries of the files, epage1a and fpage2a (the second line data files), being inserted at the corresponding columns. Efforts were made to homogenize each entry by correcting column shifts and by separating code flags from numerical data. No essential change of data was, however, made except for only one case: The v sin i data for HBC 419 was rounded off from 12.5 to 13 according to the relevant description in the text file. The file, iref (the literature references in single-column format), was reconstructed into the format of one reference per line. This and together with other two files, btext and grem, were updated by deleting page numbers and surplus blank lines. Finally, corrections have been made according to the list communicated by Dr. Herbig. August 1995 (Paul Kuin): Reformatted the documentation to standard form. V_73A.xml Catalogue of Observational Data in Galactic Star-Forming Regions 5074 V/74 Observational Data in Galactic Star-Forming Regions Catalogue of Observational Data in Galactic Star-Forming Regions V S Avedisova CDS Bull. No. 41, p. 25 ??? ??? 1992 1992BICDS..41...25A Combined data Interstellar medium Nebulae Stars, pre-main sequence The catalogue of observational data in galactic star-forming regions represents a compilation of the data from various optical, radio (in continuum and line) and infrared surveys of the galactic plane and also from papers on individual sources.
Catalog Data GLON Galactic longitude of source deg GLAT Galactic latitude of source deg sub_GLON Longitude of a subsystem deg sub_GLAT Latitude of a subsystem deg type Type of data R = radio IR = infrared M = molecular --- ID Source name --- sub_ID Designation of fine structure source --- RAh Right ascension hours (1950) h RAm Right ascension minutes (1950) min RAs Right ascension seconds (1950) s DE- Declination sign --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin DEs Declination seconds (1950) arcsec lamda Observered frequency (gHz) or wavelength (um) --- flux Flux density or antenna temperature Jy size_lim Upper or lower size limit --- hpw Half power width Halfpower width in right ascension if there are no units in 106 --- unit_hpw Units for half power width --- hpw_del Half power width in delta --- hpw_unit Unit for half-power width --- n_hpw Asterisk=hp beamwidth for hpw_del --- V Center velocity & width in LSR km/s ref Reference --- References ref_no Reference number If ref_no is blank, the line is a continuation of the previous line and the first twelve bytes are also blank. --- ref Reference --- Bibliography Ordered by Author ref Reference --- ref_no Reference number If ref_no is blank, the line is a continuation of the previous line and the first five bytes are also blank. --- Index of Sources ID Identification --- GLON Galactic longitude deg GLAT Galactic latitude deg intro.txt The CDS description N.G. Roman ADC/SSDOO 1997 Aug 06 V_74.xml Catalogue of Astrophysical Parameters of Binary Systems 5075 V/75 Cat of Astrophysical Parameters of Binary Systems Catalogue of Astrophysical Parameters of Binary Systems O Y Malkov CDS Bull. No. 42, p. 27 ??? ??? 1993 1993BICDS..42...27M Binaries, eclipsing Binaries, orbits Binaries, spectroscopic Binaries, visual Stars, double and multiple The first version of this catalog was created in 1989. The aim of this work was to provide a list of binaries with well-determined masses and other astrophysical parameters. As a great variety of new data has appeared since 1989, many new systems were added in the catalog. Data for many other systems were superseded with new ones. The catalog contains data on 144 systems. The complete list of the systems is presented in Table 1 (see below). It contains 288 identifications since we gave two designations per system. Each system in the data file fills two 114 byte-length records, the primary star is in prime.dat and the secondary one in second.dat. The data in the catalog are sorted in accordance with types of systems (in second.dat), then with decreasing of the primary's masses (in prime.dat). Each system includes star name, period of binary systems, effective temperature, mass, radius, luminosity, system type, reference code, etc.
primary star of the binary systems ID1 Name of the star --- P Period in days d SP Spectrum --- log_Te1 Log T(eff) K e_log_Te1 Uncertainty in log T(eff) K M1 Mass in solar units solMass e_M1 Uncertainty in mass solMass R1 Radius in solar units solRad e_R1 Uncertainty in radius solRad L1 Log L in solar units solLum u_L1 Uncertainty flag (:) for L1 --- e_L1 Uncertainty in log L solLum Mv1 M(v) mag u_Mv1 Uncertainty flag (:) for Mv1 --- e_Mv1 Uncertainty in Mv1 mag log_g1 Log g cm/s e_log_g1 Uncertainty in log g cm/s Rem1 Remarks code Remarks coded according to the following list: 1 = Out of the main-sequence (MS) band 2 = Probably pre-MS star 3 = Probably contact system --- secondary star of the binary systems ID2 HD/BD/other identifications --- TYPE Type of the system Type of the system coded according to the following list: 1 = Detached main-sequence eclipsing systems, B6 to M 2 = OB eclipsing systems 3 = O-type systems 4 = Detached subgiant eclipsing systems 5 = Resolved spectroscopic binaries 6 = Visual binaries 7 = Hot semidetached systems 8 = Algol systems 9 = Cool semidetached systems 10 = Contact and nearly contact systems (does not include W UMa systems) --- REF Bibliographic references See the reference list below. Table 1. Identifications of the systems included in the catalogue --------- --------- --------- -------- -------- --------- GCVS WW Dra V Pup 20173 128171 218066 ---- BS Dra PV Pup 20301 128620/1 219113 TW And CM Dra XY Pup 21985 131156 227696 V805 Aql RZ Eri RZ Pyx 24909 132742 228854 RY Aqr AS Eri VV Pyx 25833 135876 232121 BW Aqr CW Eri V701 Sco 26976 BC 139006 240208 V539 Ara TZ For V760 Sco 30050 139319 287727 SX Aur RY Gem U Sge 33088 139588 317844 TT Aur YY Gem V356 Sgr 33357 147683 334426 WW Aur Z Her V1647 Sgr 33959 150680 AR Aur RX Her CD Tau 34335 150708 HS Aur TX Her RW UMa 34364 152751 Bayer LY Aur DI Her CV Vel 35311 154676 ----- SS Boo MM Her DM Vir 35921 155876 Alp Aur ZZ Boo V624 Her Z Vul 37021 156247 Bet Aur AS Cam TT Hya RS Vul 37364 156384 Ksi Boo AD Cap VZ Hya 37513 156633 Eta Cas EM Car AI Hya 38735 156965 Alp Cen QX Car GK Hya BD 39780 158614 Alp CMa V348 Car HS Hya -------- 40183 161321 Alp CMi RX Cas KW Hya -16 6074 44691 161783 Alp CrB SX Cas RT Lac -5 1935 46052 163708 Khi Dra YZ Cas AR Lac +0 2259 48915 163930 Del Equ AO Cas CM Lac +2 1993 56429 165341 Omi2 Eri BC PV Cas UV Leo +22 3245 58713 170153 Dze Her SZ Cen RV Lib +25 5003 61421 170470 Khi2 Hya WX Cep GG Lup +32 1582 62863 170757 Del Lib CW Cep RR Lyn +32 4756 65818 173787 Bet Per DH Cep FL Lyr +39 2849 67862 175227 Gam Per EI Cep TZ Men +47 781 71581 177708 Dze Phe EK Cep UX Men +47 1350 72257 179890 Alp Vir TV Cet VV Mon +52 1579 73343 180939 Gam Vir UV Cet AR Mon +56 2783 74307 181182 XY Cet TU Mus +67 244 75747 181987 RS Cha U Oph 75920 185912 Flamsteed RZ Cha WZ Oph 77464 190020 --------- GZ CMa V451 Oph HD 79193 190786 68 Her S Cnc V1054 Oph ----- 86118 193611 70 Oph RZ Cnc BM Ori 1337 90242 193637 12 Per RT CrB EW Ori 4161 90707 198846 AI Cru V1031 Ori 4614 92109 202275 RS CVn AW Peg 6882 93486 203069 Others Y Cyg BK Peg 6980 96314 205234 ------ MY Cyg EE Peg 7551 97484 206046 ADS 10598 V382 Cyg RY Per 7700 97528 206135 CpD -60 3723 V442 Cyg AG Per 14871 100213 206821 Fu 46 V453 Cyg DM Per 16739 110379/80 207956 GL 630.1 V477 Cyg IQ Per 17034 114519 209147 HR 6426 V478 Cyg LX Per 18597 116658 209318 Kr 60 V1143 Cyg AI Phe 18925 120359 210334 L 726-8 V1765 Cyg SZ Psc 19115 121648 213631 TW Dra UV Psc 19356 123423 215835 --- SP Spectrum --- log_Te2 Log T(eff) K e_log_Te2 Uncertainty in log T(eff) K M2 Mass in solar units solMass e_M2 Uncertainty in mass solMass R2 Radius in solar units solRad e_R2 Uncertainty in radius solRad L2 Log L in solar units solLum u_L2 Uncertainty flag (:) for L2 --- e_L2 Uncertainty in log L solLum Mv2 M(v) mag u_Mv2 Uncertainty flag (:) for Mv2 --- e_Mv2 Uncertainty in Mv2 mag log_g2 Log g cm/s e_log_g2 Uncertainty in log g cm/s Rem2 Remark code (same as primary data) --- Francois Ochsenbein CDS C.-H. Joseph Lyu Hughes STX/NASA 1996 Oct 31 The original Intro file by Malkov O.Y. (1993) was used to create this ReadMe file. Author's Address: O.Yu.Malkov, Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya syt., Moscow 109017, Russia V_75.xml A Catalogue of Chromospherically Active Binary Stars 5076 V/76 Chromospherically Active Binaries A Catalogue of Chromospherically Active Binary Stars K G Strassmeier D S Hall F C Fekel M Scheck Astron. Astrophys. Suppl. Ser. 100 173 1993 1993A&AS..100..173S Stars, double and multiple Cross identifications Combined data Stars, emission Stars, variable The catalog contains 206 spectroscopic binary systems with at least one late-type component that shows Ca II H and K emission in its spectrum. These systems include the classical RS CVn binaries and BY Dra binaries. The catalog summarizes information on the photometric, spectroscopic, orbital, and physical properties of the systems as well as space motions and positions. Up to 42 "parameters" for each stellar system are listed followed by the appropriate reference to direct interested colleagues to the original papers. A comprehensive selection of further information for each star is given in the individual notes. In addition, the catalog contains a candidate list of 138 stars that have similar characteristics but are not definitely known binaries or have not had Ca II H and K emission observed. This version updates and replaces the 1988 catalog of similar information. (Strassmeier et al., 1988).
Stars always appear in order of increasing right-ascension for the epoch 2000.0. For the current version of the catalog, the literature was searched through December 31, 1991 although a few later references are included. Additionally, some entries are cited with "private communication", which make this catalog also a first-hand source. A number in parentheses behind an entry always corresponds to a reference given in the bibliography. See the 1988 publication for specific requirements and restrictions in compiling these catalogs. See the source reference for more details about this catalog. The following binary systems, which were listed in the first edition of the catalog, were not included in the present edition due to insufficient evidence for chromospheric activity: eta And 26 Aql 4 UMi nu2 Sgr tau Sgr the following stars are chromospherically active but are components in a "wide" binary and were not included. HD 25893 HD 79211 Forty three new binary systems have been included in the present edition.
Cross references num Catalog sequence number --- name Variable name "General Catalog of Variable Stars" identification or NSV = "New Catalog of Suspected Variable Stars" number. --- HD HD/HDE number --- HR HR number --- Bayer Bayer name --- Flam Flamsteed name --- DM DM number --- SAOzone SAO zone --- SAOnum SAO number --- other Identifications given by other sources ADS = Aitken Double Star. (The angle brackets,<>; indicate which of the visual components is the active binary. The parentheses, ( ), indicate the visual component or components that are included in the V-magnitude listed in File 2). GC = General Catalog, Gl = Gliese Catalog BV = Bamberg Variable, CZ = Cape Zone Star number, FK4 = Fundamental Katalog No. 4, AGK2= Zweiter Katalog der Astronomischen Gesellschaft, AGK3= Dritter Katalog der Astronomischen Gesellschaft, LDS = Luyten Double Star, OS = Otto Struve Variable, P = Prager Variable, S = Sonneberg Variable, vB = van Buren number, SVS = Soviet Variable Star, HV = Harvard Variable, Lal = Lallande Star, Boss= Boss number, BPM = Bruce Proper Motion survey number, PPM = Proper Motion catalog, 1E = First EINSTEIN catalog of x-ray sources, Ynn = Yale Catalog Volume nn number, Cnn = Cape Photographic Catalog Volume nn number. --- Photometric properties num Catalog sequence number --- name More commonly used name from table1.dat --- HD HD/HDE number + component --- magtyp Magnitude type --- V Vmax Maximum brightness in V bandpass. "pg" means that only an old photographic magnitude was available. mag u_V Uncertainty flag (:) on V --- r_V Reference for Vmax --- del Delta wave Maximum amplitude of the "wave" in V passband, due to spots, not ellipticity or reflection. CONST = photometry has been obtained but no wave has been observed. mag r_del Delta wave reference --- per Photometric period Photometric (= rotation) period, in days, derived from the light curve. Rotation periods from (v sin i) measurements are not included. If "(orb)" is given, then the photometric period is nearly the same as the orbital period in File 4. Sometimes Pphtm has been computed from the wave migration period using the relation 1/Pmigr = 1/Pphtm - 1/Porb; if so, this has been mentioned that in the individual notes. Due to the inherently irregular behavior of large starspot groups, the photometric period in all spotted stars is intrinsically variable! d r_per Reference for photometric period --- U-B < U - B > hot/cool mag r_U-B Reference for < U - B > --- B-V < B - V > hot/cool mag r_B-V Reference for < B - V > --- V-R < V - R > hot/cool mag r_V-R Reference for < V - R > --- R-I < R - I > hot/cool mag r_R-I Reference for < R - I > --- Spectroscopic properties num Catalog sequence number --- name More commonly used name from table1.dat --- HD HD/HDE and component --- spec Spectral type hot/cool Spectral type and luminosity class of the hot/cool component, respectively, separated by a slash "/". Spectral types and luminosity classes in brackets, "[ ]", are assumed. Braces, "{ }", denote the close binary in a spectroscopic triple system. --- r_spec Spectral type reference --- bin Binary nature Binary nature. SB1 = single-line spectrum SB2 = double-line spectrum SB3 = three components are seen in the spectrum (spectroscopic triple system) Y = yes, spectroscopic binary, but not yet known if the spectrum is single-or double-lined. --- r_bin Binary reference --- vsini Projected rotational velocity for hot/cool km/s r_vsini V sin(i) reference --- Caem CaII H&K emission Singly ionized calcium H and K emission. This column contains information on the strength of the emission as well as to which component the emission belongs. Absolute emission-line surface fluxes are given, if available, in the "Notes". cool = the cooler component is the emitter hot = the hotter component is the emitter both = both components show H and K emission class A, B, C, D, (E) = emission strength after Hearnshaw's scale, (see Figure 1 in Strassmeier et al. 1988) IK = 5, 4, 3, (2) = strength of the K-emission line in terms of Wilson's eye-estimated intensities on a scale from 0 (no) to 5 ("strong") emission. --- r_Caem CaII emission reference --- Halp Balmer H{alpha} line behavior abs. = "normal" absorption, em. = emission above the continuum, fld-in abs. = absorption profile "filled-in" with (presumably) chromospheric emission, strong abs. = strong absorption profile, mod. abs. = moderate absorption (this terminology is taken whenever an author used it but is equivalent to "filled-in abs."), wk abs. = weakly filled-in absorption profile (in these cases the degree of "filling-in" is not obviously visible by visual inspection but significant when a standard star spectrum is subtracted). flares = Hff flare has been observed. For further explanation, the original reference should be examined. --- r_Halp H{alpha} reference --- X X-ray luminosity (10+31 erg/s) f_x = only a flux measure in mW/m2 (erg/cm2/s) is available. 10+24W r_X X-ray reference --- rad Radio flux density mJy r_rad Radio flux reference --- Orbital elements num Catalog sequence number --- name More commonly used name from table1.dat --- HD HD/HDE and component --- per Orbital period d r_per P(orb) reference --- pervar Orbital period variability Orbital period variability. More quantitative results in terms of (dlnP/dt) are given in the individual notes. y = yes n = no --- r_pervar Period variability reference --- comp Component behind at conjunction p = primary behind s = secondary behind t = tertiary behind --- JD Heliocentric Julian date - conjunction Heliocentric Julian date of conjunction -2400000 with the (presumed) hotter star behind. If the star is not an eclipsing binary, then JD has been computed either from the time of periastron passage or, if e = 0, from the time of quadrature in order to simulate primary eclipse. d r_JD Conjunction date reference --- V0 System's center-of-mass radial velocity km/s r_V0 V0 reference --- K Semiamplitude of the hot/cool component If both stars have the same spectral class, then the more massive star is listed first. If both stars have the same mass, then the larger star is listed first. km/s r_K K reference --- paren1 parentheses Parentheses appear here only in record 155. The meaning is unknown. --- e Eccentricity --- paren2 parentheses Parentheses appear here only in record 155. The meaning is unknown. --- r_e Eccentricity reference --- omega Longitude of periastron deg r_omega omega reference --- asini Separation a sin(i) for hot/cool (a sin i) = total semimajor axis if no slash, /, is given (a1sin i)/(a2 sin i) = semimajor axis for the orbit of the hot/cool component respectively. "a =" in the (a sin i) column means, that the sum of the orbital semimajor axes is listed. If both stars have the same spectral class, then the more massive star is listed first. If both stars have the same mass, then the larger star is listed first. Braces, "{ }", denote the close binary in a spectroscopic triple system. 10+6km r_asini a sin(i) reference --- Stellar properties and general information num Catalog sequence number --- name More commonly used name from table1.dat --- HD HD/HDE and component --- dist Distance Distance in parsecs. If no reference is given, then the value has been computed from the absolute visual magnitude already given in the catalog. No interstellar absorption was taken into account. A value in brackets, [ ], has been computed from a V value itself in brackets, as explained below. pc r_dist Distance reference Dashes, "-", in a reference column mean that this entry has been computed by the authors. --- V M(V) of hot/cool components Absolute visual brightness. If no reference is given, then the value has been computed from dist. A value in brackets, [ ], is an assumption from the spectral type. mag r_V M(V) reference Dashes, "-", in a reference column mean that this entry has been computed by the authors. --- mass Masses of hot/cool components Mass in solar units of the hot/cool component respectively. A ">" indicates that (m sin^3^ i) is listed, and "f(m)" indicates that the mass-function is given. If both stars have the same spectral class, then the more massive star is listed first. If both stars have the same mass, then the larger star is listed first. (Note that all entries in the "MASSES" bytes followed by the reference "(727)" can't be found in that paper, but their orbital elements have been used to determine these entries.) A slash, "/", always separates values for the hot/cool component, respectively. If no slash is given, then the combined value is listed. solMass r_mass Masses reference Dashes, "-", in a reference column mean that this entry has been computed by the authors. --- rad Radii of hot/cool components Radius in solar units of the hot/cool component respectively. A " " indicates that (R sin i) is listed. Same convention as above for cases of identical spectral class or equal mass. A slash, "/", always separates values for the hot/cool component, respectively. If no slash is given, then the combined value is listed. solRad r_rad Radii reference Dashes, "-", in a reference column mean that this entry has been computed by the authors. --- ecl Eclipse Type of eclipse. It means: NONE = Not eclipsing, TOT = complete (total/annular) eclipses, PRTL = partial eclipses, YES = an eclipse has been observed, but it is not known if partial or total PSBL = it is possible that eclipses take place but further observations are necessary to confirm it. --- r_ecl Eclipse reference Dashes, "-", in a reference column mean that this entry has been computed by the authors. --- i Inclination Inclination of the pole of the orbital plane or of the rotation axis, in degrees. deg r_i Inclination reference Dashes, "-", in a reference column mean that this entry has been computed by the authors. --- IUE IUE archive Observed with IUE (through March 31, 1990)? --- IAU IAU Comm. 27 archive File in the IAU Commission No. 27 "Archive of Unpublished Observations of Variable Stars" (Breger 1985; Breger, Jaschek, Dubois 1990, IBVS 3422). Values in brackets, "[ ]", are assumed. Braces, "{ }", denote the close binary in a spectroscopic triple system. --- Positions and space motions num Catalog sequence number --- name More commonly used name from table1.dat --- HD HD/HDE and component --- RAh Right Ascension 2000.0 (hours) h RAm Right Ascension 2000.0 (minutes) min RAs Right Ascension 2000.0 (seconds) s DE- Declination 2000.0 (sign) --- DEd Declination 2000.0 (degrees) deg DEm Declination 2000.0 (minutes) arcmin DEs Declination 2000.0 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg dist Distance from table5.dat pc V0 Systemic Velocity from table4.dat km/s pmRA Proper motion in Right Ascension mas/yr pmDE Proper motion in Declination mas/yr r_V0 Systemic velocity reference --- X X pc Y Y pc Z Z pc U U km/s V V km/s W W km/s Candidate list num ? Number; blank indicates continuation --- id HD and other Identification --- V V magnitude, mean brightness in V passband mag chr Active Chromosphere? Active chromosphere? This column lists whether there is observational evidence for the existence of an active chromosphere or not. HK emission = CaII H and K emission lines were observed x-ray source = the star has been detected as an x-ray source H_a em. = H{alpha} line is in emission H_a fld-in = H{alpha} line is in absorption but "filled in" by (presumably) chromospheric emission ? = no observations available --- r_chr Activity reference --- bin Spectroscopic Binary system? Spectroscopic binary system? SB1 = single-lined spectrum SB2 = double-lined spectrum yes = yes, the star is a binary but more observations are needed v_r const? = constancy of measured radial velocities is questioned eclipsing = the system is an eclipsing binary ? = no observations available --- r_bin Binary reference --- note Individual notes --- References ref Reference Number --- text Text of Reference --- doc.tex LaTeX description notes.tex Notes in LaTeX refs.tex References in LaTeX Nancy Grace Roman SSDOO/ADC modified J.A. Watko ADC 1996 Aug 15 UNKNOWN UNKNOWN Supersedes V/71 V_76.xml Catalogue of the Objects in the Direction of the Small Magellanic Cloud 5078 V/78 Cat of the Objects in the Direction of the SMC Catalogue of the Objects in the Direction of the Small Magellanic Cloud M Bischoff A Florsch J Florsch J Marcout Publ. Obs. Astron. Strasbourg, Equipe "Populations Stellaires" ??? ??? 1988 1988 Combined data This catalog is an attempt to provide a definitive compilation of objects in the Small Magellanic Cloud. It contains five files: the General Catalog, Variable Stars, Miscellaneous objects, Coordinates for the equinox 2000 and rectangular coordinates in Wesselink's system, and Bibliographic references. The General Catalog contains 1975 positions, spectra, photographic and visual magnitudes, B-V, U-B, radial velocities, and numbers in various catalogs. The Miscellaneous list describes each object but gives only photographic magnitudes.
General Catalogue No Number of the star --- RAh Right Ascension hours (1975) h RAm Right Ascension minutes (1975) min DE- Declination sign (1975) --- DEd Declination degrees (1975) deg DEm Declination minutes (1975) arcmin Sp Spectrum --- m Photographic magnitude mag V Visual magnitude mag B-V B-V color index mag U-B U-B color index mag RV Radial velocity km/s Ref References --- Id Identification --- Rem Remarks --- Variables No Number of star --- RAh Right ascension (1975) h RAm Right ascension (1975) min DE- Declination sign (1975) --- DEd Declination (1975) deg DEm Declination (1975) arcmin max Magnitude at maximum mag min Magnitude at minimum mag Per Period d Ref Reference --- Id Identifications --- Rem Remarks --- Objects No Number of the object --- RAh Right ascension (1975) h RAm Right ascension (1975) min DE- Declination sign (1975) --- DEd Declination (1975) deg DEm Declination (1975) arcmin m Photographic magnitude mag RV Radial velocity km/s Dim Size (includes the unit) --- stars Number of stars --- Obj Associated objects --- Ref References --- Id Identification 1 --- Rem Remarks --- Rectangular Coordinates No Number of the star --- RAh Right ascension hours h RAm Right ascension minutes min DE- Declination sign --- DEd Declination degrees deg DEm Declination minutes arcmin ksi ksi in Wesselink's system --- eta eta in Wesselink's system --- refs.txt Bibliography James E. Gass SSDOO/ADC 1998 Oct 22 V_78.xml Membership of Low-Mass Stars in the Open Cluster Alpha Persei 5080 V/80 Low-Mass Stars' Membership in OC Alpha Persei Membership of Low-Mass Stars in the Open Cluster Alpha Persei C F Prosser Astron. J. 103 488 1992 1992AJ....103..488P I/68A : Positions, Proper Mot 1981 Stars Near Alpha Per (Fresneau 1980) References can be found in the file refs.txt. Clusters, open Stars, masses Proper motions Spectroscopy Photometry, BV This catalog contains the tabulated results of a combined astrometric, photometric, and spectroscopic search for low-mass members in the intermediate-age open cluster Alpha Persei. It contains information on 132 new members and likely members, and 16 uncertain members of Alpha Per. The new membership information suggested to the author a revised age of the cluster to approximately 8 E+7 yr. Tabulated data include AP number, VBI photometry, 1950 coordinates, relative proper motions with errors, H-alpha equivalent widths, and spectral type. Included are the individual membership determinations, based on H-alpha emission, spectral type, and echelle spectra data. The photometric data were obtained with the Lick Obs. 1-m Nickel Telescope using a TI 500x500 pixel CCD in B, V, and I bands. Low dispersion CCD spectra centered on H-alpha for candidates whose V-I photometry indicated likely membership using the Lick 1-m Nickel and 3-m Shane telescopes. High-dispersion echelle spectra were obtained for many bright candidates using the Hamilton echelle spectrographic with the Shane and Coude auxiliary telescopes.
van den Bergh & Sher (1960) found from studying several open clusters that in general the faint end of the cluster luminosity function decreased or remained constant down to the level of observation. If true, the observed cluster luminosity functions are unable to account for the luminosity function of nearby field stars which increases to faint magnitudes. One possible solution is that additional unidentified low-mass stars exist in most (or all) open clusters. Recent studies in the Hyades (Weis & Hanson 1988, Griffin et al. 1988, Stauffer 1982), Pleiades (Stauffer et al. 1991, Prosser et al. 1991), and Praesepe (Mermilliod et al. 1990, Jones & StauAlphaer 1991) have identified faint candidate members. It is the aim of this study to determine the existence, and some of the properties, of the low-mass membership in the open cluster Alpha Persei. Alpha Per was chosen for study because of the limited information on low-mass membership, because it is nearby (which enables both proper motion analysis and observation of low-mass candidates), because no other clusters of the same relatively youthful age have been studied completely, and because of the existence of the photographic plate material needed for the proper motion analysis. After a brief review of the history and previous work in this cluster, the proper motion survey of this study is described. This is accompanied by a description of the CCD photometry and spectroscopy programs employed to aid in identifying cluster members. A review of current information on previous members and possible members is also given, followed by a section presenting the new members and candidate members found in this study. An analysis of some cluster properties including luminosity function, age, spatial distribution of members, reddening, H-alpha emission strengths, and rotational velocity distribution is presented. Finally, the last section provides a general review of the results found in Alpha Per.
Table 4: HE candidates (Heckmann et al. 1956) HE Star identification --- HEn Heckmann's star identification numbers, followed by an "N" if it is a non-member. --- V V magnitude Photometry from Mitchell (1960). Identification of nonmembers in table 4 was usually based on star's photometry and radial velocity. mag u_V V magnitude uncertainty flag --- B-V B-V color index mag BDz BD zone --- BDno BD Number within zone --- BDs BD number suffix --- RAh Right ascension (1950) Coordinates determined from the x,y coordinates in arcsec given by Heckmann et al. (1956). h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec RVKr Radial velocity from Kraft km/s RVo Other radial velocity km/s e_RVo Error in other radial velocity km/s limit Limit indication for rot. velocity --- Vrot Rotational velocity from echelle spectra Radial and rotational velocities in table 4 are from a variety of sources, rather than from this study. km/s u_Vrot Rotational velocity uncertainty flag --- ref_1 Reference 1 1). Petrie and Heard (1970). 2). Stauffer et al. (1985). 3). Stauffer et al. (1989). 4). Kraft (1967a). 5). This study, Hamilton spectrograph. 6). Abt et al. (1990). 7). Morse et al. (1991). 8). Morrell and Abt (1991). 9). HE 441 = HD 20510. 10). HE 601: V0-MV=14.4, Crawford and Barnes (1974). 11). Mermilliod (1991). --- ref_2 Reference 2 --- mphot HE membership from photometry --- mesche HE membership from echelle spectra --- mli HE membership from LI --- mfinal Final HE membership determination --- notes Notes --- Table 6: Fresneau's suggested HE members HE Star identification --- V V magnitude mag B-V B-V color index mag V-I V-I color index mag v Number of V observations --- b Number of B observations --- i Number of I observations --- BDz BD zone --- BDno BD Number within zone --- RAh Right ascension (1950) Coordinates from Heckmann et al. (1956). h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Fprob Fresneau's membership probability Probability of membership in Alpha Persei cluster from Fresneau (1980). --- mBVI Membership based on BVI Fresneau's membership status based on BVI photometry. --- muvby Membership based on uvby-beta photometry by Trullols et al. (1989) Trullols et al. (1989) obtained uvby-beta photometry for a number of these stars and assigned this membership status for them. --- RV Radial velocity from echelle spectra Velocity information in Table 6 is mostly from the echelle spectra obtained in this study. km/s e_RV Error in radial velocity km/s limit Limit indication for rot. velocity --- Vrot Rotational velocity from echelle spectra km/s u_Vrot Rotational velocity uncertainty --- mfinal Final HE membership determination --- notes Notes --- Table 10: New AP membership information AP AP number To avoid confusion, the author has given new cluster members and candidate cluster members the designation of AP stars numbered consecutively to follow the lists of Stauffer et al. (1985,1989). --- V V magnitude The photometric data were obtained with the Lick Obs. 1-m Nickel Telescope using a TI 500x500 pixel CCD in B, V, and I bands. mag B-V B-V color index mag V-I V-I color index mag v Number of V obs. --- b Number of B obs. --- i Number of I obs. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec pmX Relative proper motion in X direction as/a pmY Relative proper motion in Y direction as/a e_pmX Proper motion error in X direction cas/a e_pmY Proper motion error in Y direction cas/a EW H-alpha equiv. width (angstroms) dnm Sp MK Spectral Type --- mphot phot. membership determination The author has used the V-I color to separate cluster stars from the background field. The determination was based on plotting V-I vs. V. --- mhalph H-alpha membership determination Low dispersion CCD spectra centered on H-alpha for candidates whose V-I photometry indicated likely membership were obtained using the Lick 1-m Nickel and 3-m Shane telescopes. Stars showing definite emission at low dispersion form a well defined sequence in a plot of V vs. pMK. Stars falling below this sequence have spectral types too early for their apparent magnitudes. Many of the stars falling below the cluster sequence are late-type (K, early M) stars, with weak H alpha absorption. Some stars along the sequence are H alpha filled, and may be stars having weaker H alpha emission that is not strong enough to result in a noticeable emission feature at this resolution. Y = emission, F = filled, WA = weak absorption, N = no emission --- mspect Spectral membership determination (See note on mhalph). The presence or absence of H alpha emission alone is not adequate for membership determination. The spectral type is an aid based on the V vs. pMK sequence and the H alpha observations are a confirming or secondary aid. --- mesche Echelle spect. determination A large fraction of the bright candidates were observed using the Hamilton echelle spectrograph on the 3m Shane and Coude Auxilliary telescopes. These were used to measure radial and rotational velocities. Slow rotators (Vrot <= 20 km/s) with radial velocities within approx. 2 km/s of the cluster mean were considered to be members. --- mfinal Final membership determination --- notes Notes Additional notes related to the final cluster membership determination. MMT means that a low-dispersion MMT spectrum at H alpha was obtained. --- Table 11: Velocities of new AP stars AP AP number To avoid confusion, the author has given new cluster members and candidate cluster members the designation of AP stars numbered consecutively to follow the lists of Stauffer et al. (1985,1989). --- V V magnitude The photometric data were obtained with the Lick Obs. 1-m Nickel Telescope using a TI 500x500 pixel CCD in B, V, and I bands. See source reference for details of the photometric reduction. mag B-V B-V color index mag V-I V-I color index mag RV Heliocentric radial velocity km/s e_RV Error in radial velocity km/s Vrot Rotational velocity (Vsini) km/s LI Presence of Li 6707 line Indicates presence (and/or relative strength) of Li 6707 absorption line for the new AP stars from the high-dispersion spectra. This is considered a supporting piece of evidence for cluster membership. --- mesche Membership based on echelle spectra Indicates whether or not radial velocity and rotational velocity from echelle spectra suggest cluster membership. (See note on mesche for table 10 above). --- Notes Notes on binary status, spectrum, velocity --- Prosser.tex LaTeX Document (in lyxtex) lyxtex.tex Lyxtex macros based on Psizzl refs.txt References from the source publication James E. Gass ADC/SSDOO 1997 Jun 04 UNKNOWN UNKNOWN [ADC] 4-Jun-1997: The tables were extracted from the lyxtex files provided by the author. This necessitated reformatting to align columns and replace some non-ASCII characters. The parentheses around velocity error values in table 6 were removed. [ADC] 4-Jun-1997: Coordinates in table 4 were computed by author from x,y coordinates of Heckmann et al. (1956). ADC changed two entries as follows: HE 756 Dec changed from 48d 05' 60." to 48d 06' 00." HE 861N Dec changed from 46d 45' 60." to 46d 46' 00." V_80.xml Taxonomy of Barium Stars 5081 V/81 Taxonomy of Barium Stars Taxonomy of Barium Stars P K Lu Astron. J. 101 2229 1991 1991AJ....101.2229L Spectroscopy Stars, late-type Stars, barium Image-tube spectra and photometric observations for 389 bariums stars have been used to determine spectral classification, barium intensity, radial velocity, luminosity, and kinematical properties. The objective of this study is to obtain a homogeneous dataset for analyzing barium characteristics in uniform fashion.
The objective of this study is to obtain a homogeneous dataset for analyzing barium characteristics in uniform fashion. The analyses show that barium stars appear to have young to old disk kinematics based upon whether they are Ba weak or Ba strong. The Ba II line (4554A) is also identifiable in dwarf stars; these dwarf barium stars are small in number and weak in intensity. The analyses of the kinematics, luminosities, U,V,W velocity distributions using image-tube radial velocities and statistical parallaxes using proper motions and upsilon components show that the weak barium stars generally tend to have smaller velocity dispersion, and brighter apparent magnitudes at about same distance compared to strong Ba stars, and thus lower luminosity. The solution for the mean spectroscopic distances, the z-scale height distances and reduced proper motions also confirm the this finding.
The data Seq Sequential number. --- HD/DM Durchmusterung or HD designation BD=Bonner Durchmusterung, CD=Cordoba, CP=Cape, SD=Suedlicher BD MFU=MacConnell, Frye, Upgren, 1972, AJ 77, 384 default is HD --- Source Source and remarks b new BaII from Bidelman objective-prism survey (1981,1983) AJ 86, 553; AJ 88, 1182 h from Houk catalogues (MSC Vol. 1-4) k Keenan semi-barium stars (Ba=0.3-0.9) (1980) K Keenan and McNeil (1989) ApJS 71, 245 l from Lu image-tube spectra ! HD 20644, BS 999; not HD60649 as listed Keenan and McNeil, 1989, ApJS 71, 245) < star listed in the Perkins Catalog of Revised MK Types (Keenan and McNeil, 1989, ApJS 71, 245) ^ component velocity available in Catchpole et al (1977) MNRAS 181, 391 * MFU 112 = #163 (Paper I); + radial velocity standard --- RAh Right Ascension, B1900.0 h RAm Right Ascension (minutes) min DE- Declination sign --- DEd Declination, B1900.0 deg DEm Declination (minutes) arcmin MK Spectral type - no luminosity class given in MSC * HD 13551 listed as weak line F3 by Houk (MSC v1) HD 22772 has Ib luminosity from DDO HD 76225 composite spectral types F7/G+A(p Sr) by Houk (MSC v3) HD 87080 listed as weak line star by Houk (MSC v3); Class V from DDO HD 87761 Class V from DDO, Class II from Houk (MSC v1) HD 123585 listed as F7 V weak line and strong Sr by Houk (MSC v2) HD 130255 Suggested as dwarf barium by Keenan HD 150862 has composite spectral types of V+a (p Sr) by Houk (MSC v3) HD 202400 has Ap Sr spectral type by Houk (MSC v1) --- BaClass Ba intensity class --- BaCode Ba intensity code c certain Ba stars in MFU m marginal Ba in MFU n non-barium stars (Paper I) --- u_BaClass Uncertainty flag (:) on BaClass --- m48 DDO m48 mag 45-48 DDO color 45-48 mag 42-45 DDO color 42-45 mag 41-42 DDO color 41-42 mag 38-41 DDO color 38-41 mag o_m48 No. of observations in DDO system m from McClure and Forrester (1981) Publ. DAO 15, 439 d from Dean (1981) South. Africa Astron. Obs. Circ. 6, 10 --- Vmag V-mag. (all BVRI are photoelectric). mag B-V B-V colour index mag V-R V-R colour index mag R-I R-I colour index mag o_Vmag No. of observations in BVRI system --- pmRA Proper motion in RA mas/yr pmDE Proper motion in Dec mas/yr RadVel Radial velocity km/s r_RadVel Reference of Radial velocity source of radial velocity: a from Abt and Biggs (1972) (catalogue III/4/) b from Beavers and Eitter (1986) ApJS 62, 147 B from Barbier-Brossat and Petit (1986) A&AS 65, 59 c from Catchpole, Robertson, and Warren (1977) MNRAS 181, 391 C from Yale cross-corr. (Lu, 1985) IAU Coll. 88, 207 D form 2D-Frutti spectra i image-tube velocity j from Jorissem and Mayor (1988) A&A 198, 187 --- u_RadVel Uncertainty(:)/variability(v) on RadVel --- Mv Absolute magnitude derived from spectral type and luminosity class mag Dist Spectroscopic distance pc GLON Galactic Longitude, l(II) values present only when kinematical data are available deg GLAT Galactic Latitude, b(II) deg U U-velocity km/s V V-velocity km/s W W-velocity km/s Zdis Z-scale height distance in pc pc Hm Reduced proper motion in magnitude the reduced proper motion is defined by: Hm = Vmag + 5 log(pm) - 5 = Mv + 5 log(T) - 3.379 where T is the tangential velocity (expressed in km/s) and pm the total proper motion (expressed in arcsec/yr) mag SAO SAO number --- Remarks Remarks --- Francois Ochsenbein CDS 1995 Apr 24 UNKNOWN UNKNOWN * Feb 7, 1995: prepared by Nancy G. Roman [ADC] and Philippe Lu [Western Conn. St. U.] * 25-Apr-1995: standardized at CDS V_81.xml Strasbourg-ESO Catalogue of Galactic Planetary Nebulae 5084 V/84 Strasbourg-ESO Catalogue of Galactic Planetary Nebulae Strasbourg-ESO Catalogue of Galactic Planetary Nebulae A Acker F Ochsenbein B Stenholm R Tylenda J Marcout C Schohn European Southern Observatory -- ISBN 3-923524-41-2 ??? ??? 1992 1992ESOPN...1....1A Planetary nebulae The electronic version of the catalogue referenced above includes 1143 true and probable planetary nebulae (Table 1 of publication); 347 objects which status is still unclear were classified among the "possible" planetary nebulae (file pospn.dat, Table 2 of publication); and 330 objects have been rejected (file notpn.dat, Table 3 of publication). The designation system of the planetary nebulae of this catalogue follows the recommendations of IAU Commission 5 (Astronomical Nomenclature) with the structure: PN Glll.l+bb.b where PN means "Planetary Nebula", G stands for "Galactic Coordinates", and lll.l+bb.b stand for the galactic longitude and latitude respectively, truncated to one decimal place. The designations following this system appear in the columns labelled "PNG" in the tables described below, where the "PN G" prefix has been stripped. Data concerning the 1143 true and probable planetary nebulae (part II of the publication) have been grouped in a set of related tables described below, all sorted by the "PNG" column. Note that, unlike the printed volume, only the bibliographic references corresponding to data listed in the tables are provided here, in the "refs.txt" file. Copies of the complete catalogue, including the Finding Charts (Part I) can still be ordered at the ESO Information Service, Karl-Schwarzschildstr. 2, D-85748 Garching bei Muenchen, Germany, at a price of DM 135.
Discoverers, Designations, and Positions of True and Possible Planetary Nebulae PNG Designation of the Galactic Planetary Nebula --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec qualPos Accuracy on the 1950 Position: a if RA originally only given to 0.1min d if DE originally only given to 0.1arcmin or worse * if both 'a' and 'd' --- refPos Reference of position --- Name Main designation --- PK Designation in PK67 --- IRAS Designation in IRAS catalogue --- Disc Discoverer name and publication year --- Idents Other names separated by commas --- Diameters of PN (optical and radio) PNG Designation of the Galactic Planetary Nebula --- l_oDiam Limit flag on oDiam --- oDiam Optical diameter arcsec u_oDiam Uncertainty flag (:) on oDiam --- r_oDiam References for oDiam --- l_rDiam Limit flag on Radio diameter --- rDiam Radio diameter arcsec u_rDiam Uncertainty flag (:) on oDiam --- r_rDiam Reference on Radio diameter --- Distance estimations Statistical distances PNG Designation of the Galactic Planetary Nebula --- Method Method used for distance determination number=1 This field is blank for file "dista.dat" (statistical distances); for file "dist.dat", the following symbols are used to describe the method: 'C' from cluster membership 'D' from dust 'E' from local extinction study 'K' from kinematical studies 'M' mean value from a compilation of individual distances 'S' from spectroscopic parallax of binary companions 'W' from wind 'X' from a comparison of tangential and radial expansions --- Dist1 Lower distance if l_Dist is '-' kpc l_Dist '-' if Dist1 is a lower limit; '<' or '>' apply to Dist. --- Dist Distance in kiloparsecs. kpc u_Dist Uncertainty flag on Dist --- r_Dist Reference of Dist determination. --- H-beta fluxes PNG Designation of the Galactic Planetary Nebula --- log(Fbeta) log of flux in H-beta mW/m2 e_log(Fbeta) Mean error on log(Fbeta) mW/m2 r_log(Fbeta) References --- Line intensities results PNG Designation of the Galactic Planetary Nebula --- ObsLabel Observation name (includes the date) --- LineRef Line taken as reference (value=100): 'a'=H-alpha (6563), 'b'=H-beta (4861) --- I4686 Line intensity of HeII at 468.6nm --- u_I4686 Uncertainty flag on I4686 --- I4363 Line intensity of [OIII] at 436.3nm --- u_I4363 Uncertainty flag on I4363 --- n_I5007 '*' if the measurement refers to 495.9nm because 500.7nm line is saturated --- I5007 Line intensity of [OIII] at 500.7nm --- u_I5007 Uncertainty flag on I5007 --- I5876 Line intensity of HeI --- u_I5876 Uncertainty flag on I5876 at 587.6nm --- I6563 Line intensity of H-alpha at 656.3nm --- u_I6563 Uncertainty flag on I6563 --- I6584 Line intensity of [NII] at 658.4nm --- u_I6584 Uncertainty flag on I6584 --- n_I6717 'B' if line is blended --- I6717 Line intensity of [SII] at 671.7nm --- u_I6717 Uncertainty flag on I6717 --- n_I6731 'B' if line is blended --- I6731 Line intensity of [SII] at 673.1nm --- u_I6731 Uncertainty flag on I6731 --- IUE observations log PNG Designation of the Galactic Planetary Nebula --- IUEname Name as found in the IUE Merged Log --- 1950Pos Position as found in the IUE Merged Log --- ObsDate Date and time (hours, minutes) of the Observation --- OType Object class as found in the IUE Merged Log --- Camera designation, LW=Long Wavelength, SW=Short Wavelength --- Image identification of the Observation --- IRAS Point Source Catalogue fluxes PNG Designation of the Galactic Planetary Nebula --- IRAS IRAS source name --- RAhIRAS Hours RA, equinox 1950.0, epoch 1983.5 h RAmIRAS Minutes RA, equinox 1950.0, epoch 1983.5 min RAdsIRAS Seconds RA, equinox 1950.0, epoch 1983.5 ds DE-IRAS Sign Dec, equinox 1950.0, epoch 1983.5 --- DEdIRAS Degrees Dec, equinox 1950.0, epoch 1983.5 deg DEmIRAS Minutes Dec, equinox 1950.0, epoch 1983.5 arcmin DEsIRAS Seconds Dec, equinox 1950.0, epoch 1983.5 arcsec Major Uncertainty ellipse major axis arcsec Minor Uncertainty ellipse minor axis arcsec PosAng Uncertainty ellipse position angle number=1 the IRAS flux qualities are 1 = upper limit 2 = moderate quality 3 = high quality deg NHcon Number of times observed --- Fnu12 Average non-color corrected flux density, 12um Jy Fnu25 Average non-color corrected flux density, 25um Jy Fnu60 Average non-color corrected flux density, 60um Jy Fnu100 Average non-color corrected flux density, 100um Jy q_Fnu12 Flux density quality, 12um number=1 the IRAS flux qualities are 1 = upper limit 2 = moderate quality 3 = high quality --- q_Fnu25 Flux density quality, 25um number=1 the IRAS flux qualities are 1 = upper limit 2 = moderate quality 3 = high quality --- q_Fnu60 Flux density quality, 60um number=1 the IRAS flux qualities are 1 = upper limit 2 = moderate quality 3 = high quality --- q_Fnu100 Flux density quality, 100um number=1 the IRAS flux qualities are 1 = upper limit 2 = moderate quality 3 = high quality --- Near infra-red observations PNG Designation of the Galactic Planetary Nebula --- Jmag Magnitude in J filter (1.25um) mag l_Hmag Limit flag on Hmag --- Hmag Magnitude in H filter (1.65um) mag l_Kmag Limit flag on Kmag --- Kmag Magnitude in K filter (2.22um) mag l_Lmag Limit flag on Lmag --- Lmag Magnitude in L/L' filter (3.5/3.8um) mag n_Lmag the apostrophe indicates the L' filter --- Class Class based on the near-IR number=1 The classes indicate the major source of near-IR emission: N: from the nebular gas D: from the dust S: from a star, either the exciting star or a companion P: Possibly proto-planetary nebula --- PhotRef References for JHKL --- SpRef References describing the Spectrum --- Radio observations PNG Designation of the Galactic Planetary Nebula --- l_Rad2cm Limit flag on Rad2cm --- Rad2cm Radio flux density at 2cm (14.7GHz) mJy r_Rad2cm Reference of Rad2cm --- l_Rad6cm Limit flag on Rad6cm --- Rad6cm Radio flux density at 6cm (5GHz) mJy u_Rad6cm Uncertainty flag on Rad6cm --- r_Rad6cm Reference of Rad6cm --- Radial and Expansion Velocities PNG Designation of the Galactic Planetary Nebula --- RVel Radial Velocity km/s e_RVel Mean error on RVel km/s r_RVel Source of the Radial Velocity --- l_ExpVel Limit flag on ExpVel --- ExpVel Expansion velocity [OIII] km/s u_ExpVel Note on ExpVel number=1 The '*' indicates that the value is derived from another ion (neither [OIII] nor [NII]) --- r_ExpVel Source of ExpVel --- n_ExpVel Note on the elements number=2 This flag has the following meaning: '+' when expansion velocity from other ions are given in the reference '-' when no value was given in the source --- l_ExpVel2 Limit flag on ExpVel2 --- ExpVel2 Expansion velocity [NII] km/s u_ExpVel2 Note on ExpVel2 number=1 The '*' indicates that the value is derived from another ion (neither [OIII] nor [NII]) --- r_ExpVel2 Reference of ExpVel2 --- n_ExpVel2 Note on the elements number=2 This flag has the following meaning: '+' when expansion velocity from other ions are given in the reference '-' when no value was given in the source --- Data concerning Central Stars of PN PNG Designation of the Galactic Planetary Nebula --- AG82 Name in ref. AG82 (Acker et al., Publ. Speciale CDS 3, 1982) --- Umag Johnson's U filter mag. of central star mag l_Bmag Limit flag on Bmag --- Bmag Johnson's B filter mag. of central star mag l_Vmag Limit flag on Vmag --- Vmag Johnson's V filter mag. of central star mag Quality Accuracy of the photometry number=1 The Quality are defined as follows: A: mean error < 0.10 B: 0.10 < mean error < 0.25 C: 0.25 < mean error < 0.5 D: 0.5 < mean error P: derived from photographs; mean error about 1mag. --- PhotRef References of Photometry --- Remarks Remarks on Photometry --- Sp Spectral type of central star --- r_Sp Reference of Spectral type --- Sp2 Other spectral classification --- r_Sp2 Reference of Sp2 --- Sp3 Other spectral classification --- r_Sp3 Reference of Sp3 --- Names Various designations of the Central Star separated by a semi-colon (;) --- Notes and remarks about some nebulae PNG Designation of the Galactic Planetary Nebula --- Text Text of the note --- Possible PN (table 2) Name Usual name --- n_PK The '*' indicates that PK was not published in the PK67 reference --- PK Designation in PK67 (or later, see n_PK) --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin GLON Galactic longitude deg GLAT Galactic latitude deg Class Class of the object number=1 the class has the following meaning: U = no spectrum could be detected H = faint object highly reddened showing a weak H-alpha emission H2? = faint object showing IRAS colours typical of a HII region *? = object with a faint continuum ** = object of unclear status with a well known emission line spectrum PN = possibly high or normal excitation planetary nebula PPN = proto-planetary nebula LE = low-excitation nebula --- OtherNames separated by a comma (,) --- Objects rejected as PN (table 3) Name Usual name number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. --- n_PK The '*' indicates that PK was not published in the PK67 reference number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. --- PK Designation in PK67 (or later, see n_PK) number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. --- RAh Right Ascension 2000 (hours) number=1 coordinates are blank when several PK designations have been assigned to the same PN, as e.g. PK 358-1 1 and PK 358-1 3 h RAm Right Ascension 2000 (minutes) number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. min DE- Declination 2000 (sign) number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. --- DEd Declination 2000 (degrees) number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. deg DEm Declination 2000 (minutes) number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. arcmin GLON Galactic longitude number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. deg GLAT Galactic latitude number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. deg Notes Notes concerning the object (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. number= (a) see Acker et al., 1987, A&AS 71, 163 (b) see Acker & Stenholm, 1990, A&AS 86, 219 (c) see Acker et al., 1991, A&AS 87, 499 Note 1 on Al 2-E: this PK number (359+ 3 4) was first given to the object Wray 11-88 by Allen in 1979 (Obs. 93, 83) and then used by MacConnel in 1983 (Vatican Obs. Publ. 2, n.5, 63). The object Wray 17-88 was not detected as having any emission line and is this not a PN. Kohoutek in 1983 gives the designation 359+3 4 to the object Al 2-E found by Allen and this should be used, although Allen himself gives 359+3 5. --- refs.txt References Francois Ochsenbein CDS 1994 Dec 21 V_84.xml Stellar Mass Catalogue. Preliminary Version 5085 V/85 Stellar Mass Catalogue Stellar Mass Catalogue. Preliminary Version A N Belikov Bull. Inf. CDS 47 9 1995 1995BICDS..47....9B Stars, masses The catalogue includes binary stars for which dynamical masses of components has been published in 1969 - 1988. It doesn't contain other compilation catalogues that were published in this two decades and uses original data papers only. It collects masses defined by direct, dynamical methods only (without use of mass-luminosity, mass-radius, mass-spectrum and similar relations). The work was supervised by Dr O. Malkov.
The catalogue Name Principal name of the system --- OtherID Secondary identifier of the system --- M1 Mass of primary component solMass e_M1 Mean error on M1 solMass M2 Mass of secondary component solMass e_M2 Mean error on M2 solMass Method Method of mass determination number=1 Methods of mass determination: S - methods for double lined spectroscopic binaries: The inclination of the system are derived from : S0 resolved light curve; S1 visual orbit; S2 speckle-interferometry; S3 polarimetry. V - methods for visual binaries: Photographic magnitude difference V0 is known; V1 is assumed to be zero; V2 is calculated from visual magnitudes and spectra; V3 is calculated from visual magnitudes and difference visual and photographic photocentric semimajor axes; V4 is known from speckle - interferometry; V5 is calculated from J,H,K magnitude differences. R - methods for resolved spectroscopic binaries: R0 orbital parallax used. R1 trigonometric parallax used. --- Note explained in note number=5 Individual Notes: a authors calculated all needed parameters, but didn't calculate final masses. b the trigonometric parallax used too. c authors used dynamic parallax to calculate sum of mass, but the system has trigonometric parallax the same. Authors calculated all needed parameters, but didn't calculate final masses. d authors used dynamic parallax to calculate sum of mass but the system has trigonometric parallax the same. 1 the second of this pair is the intrinsic variable star . 2 to determine mass ratio authors used self-determined radial velocities. 3 with mass ratio from Wilson & Devinney , ApJ 182, 539, 1973 4 the final stage of the B-type W UMa configuration 5 used orbit from Lippincott S.L., 1981, PASP 93, 376 6 used orbit from Russell & Gatewood, 1983, PASP 96, 429 7 a system between Roche-lobe filling stage of case C (post-helium flash) mass transfer 8 1) the primary is near filling its Roche lobe; 2) intrinsic activity is detected; 3) a member of NGC 752. 9 the secondary is intrinsic variable of delta Scuti type. 10 these system is a member of open cluster NGC 6231 of the Sco OB1 association. 11 sp.elements from Struve & Gratton, 1948, ApJ 108, 497 12 sp.elements from Struve & Zetergi, 1959, ApJ 130, 789 13 sp.elements from King & Hilditch , 1984, MNRAS 209, 645 14 this system is passing through a transition state from a semidetached configuration, reached via case A mass transfer episode to become an evolved and deep-contact A-type W UMa system. 15 UV Cet is B - component of L726-8(A+B). 16 using sp.elements by Harper W.E., Pearce J.A., Petrie R.M., Mckellar A., JRASC 29, 411, 1935 17 using sp.elements by Popper D.M., ApJ 166, 366, 1971 18 primary component is the beta-Cepheid star. 19 Algol-type eclipsing binary with an evolved and less-massive secondary component (must be filling it's Roche lobe) 20 this system has more than two stars (from anomalous large total mass) maybe. 21 the secondary has evolved G9 spectrum. 22 the system has third component of A7V spectrum. 23 the system has third component. 24 the system has third component of K5 spectrum. --- AAAref Reference from AAA number=2 number of the paper in Astronomy and Astrophysics Abstracts, made of Volume . Section . Paper number The references are explained in file "refs.dat" --- System Type of system number=3 Types of system abbreviations, the colon (:) indicates an uncertainty: Al Algol-type star c contact system ce evolved contact system d detached system dn dwarf nova fl flare star nc near contact system p.RS precursor of the RS CVn-type system R R CMa-type star RS RS CVn-type star S W Ser-type star sd semidetached system W W UMa-type star WA W UMa-type star,type A WB W UMa-type star,type B WR binary system with Wolf-Raet star WW W UMa-type star,type W --- Sp Spectral types of the two stars number=4 Spectra abbreviations: e. early m. middle l. late ? unknown spectrum (Sp) questionable spectrum + division of primary and secondary component spectra ; division of composed spectrum of system and component's spectra - uncertainty in spectral class / uncertainty in luminosity class --- References AAAref Reference as in "catalog.dat" --- Text of reference --- Francois Ochsenbein CDS 1995 Jul 19 UNKNOWN UNKNOWN The decimal points have been added where necessary. V_85.xml Analysis of Archival Data For Cool Dwarfs. II. A Catalog of Temperatures 5087 V/87 Temperatures of Cool Dwarfs Analysis of Archival Data For Cool Dwarfs. II. A Catalog of Temperatures B J Taylor PASP 106 452 1994 1994PASP..106..452T Analysis of Archival Data For Cool Dwarfs. II. A Catalog of Temperatures B J Taylor PASP 107 734 1995 1995PASP..107..734T Photometry, Cousins Effective temperatures The file contains values of Cousins R-I and theta [= 5040/T(eff)] for 497 F-K stars which are on or near the main sequence.
Paper II contains the original version of the catalog, while Paper VI contains a supplement. It is believed that the combined database in the two papers is complete for data published as of the end of 1993.
The catalog of R-I and theta prefix "vB" for Hyades stars, "Tr" for Coma stars --- BDsign "+" or "-" for BD stars, blank otherwise --- bd/hd Catalog number (HD if no other labeling) --- cmpnt For binaries: "A" if primary, "B" if secondary --- W "W" for number in Woolley et al. 1970 catalog --- hr/w HR number or Woolley et al. catalog number --- (R-I)c Cousins R-I mag sigma_c Standard deviation for Cousins R-I mag theta 5040/T(eff) --- sigma_t Standard deviation for theta --- com Comment letter --- Benjamin J. Taylor Brigham Young U. 1995 Aug 22 If there are comments or questions, please contact: Benjamin J. Taylor taylorb@astro.byu.edu Physics and Astronomy Department, ESC Tel.: 801-378-2233 Brigham Young University FAX: 801-378-2265 Provo, UT 84602 V_87.xml Analyses of Archival Data for Cool Dwarfs. V. an Annotated Catalog of Averaged Values of [Fe/H] 5088 V/88 Averaged [Fe/H] for Cool Dwarfs Analyses of Archival Data for Cool Dwarfs. V. an Annotated Catalog of Averaged Values of [Fe/H] B J Taylor PASP 106 704 1994 1994PASP..106..704T Analyses of Archival Data for Cool Dwarfs. V. an Annotated Catalog of Averaged Values of [Fe/H] B J Taylor PASP 107 734 1995 1995PASP..107..734T Abundances, [Fe/H] Stars, dwarfs Stars, late-type This file contains mean values of [Fe/H] (with rms errors) for 495 F-K stars which are on or near the main sequence. Literature references are given for the contributing values of [Fe/H].
In addition to Papers V and VI, this catalog draws on a review paper by the author on the SMR problem. If a star of interest for that problem appears without a value of [Fe/H] in Paper V, it is listed in the review paper and is also listed here with a designation "V." For all but two of these stars, mean values of [Fe/H] are given here. For the exceptions (HD 3765, HD 32147), low-resolution data suggest that [Fe/H] is substantially higher than published high-resolution results indicate (see the review paper).
The [Fe/H] catalog prefix "vB" for Hyades stars, "Tr" for Coma stars --- BD-cd "+" or "-" for BD stars, blank otherwise --- bd/hd Catalog number (HD if no other labeling) --- bin-cd Binary component or other note For binaries: "A" if primary, "B" if secondary. For single stars: "V" denotes VSL star or possible SMR star, and "C" denotes a comment --- com Comment number (see "comment.dat") 1 The D index is smaller than predicted from [Fe/H] (see 1994, PASP, 106, 600) 2 [Fe/H] may be below the catalog limit (see 1994, PASP, 106, 590) 3 See reference 221 for an alternative value of [Fe/H] 4 A reference 221 datum is included (compare refs. 221 and 570 for HD 155885/6) --- W "W" for number in Woolley et al. 1970 catalog --- hr/w HR number or Woolley et al. catalog number --- fe/h Mean value of [Fe/H] in dex --- sigma Standard deviation [Fe/H] in dex --- nu Degrees of freedom for standard deviation --- nref Number of references (max = 10) --- refs Reference numbers (see file "refs.dat") --- Reference numbers, literature sources no Reference number (see file "fehd.dat") --- l If reference requires more than 1 line, this byte contains the total number of lines for the reference. --- ref Literature reference in "PASP" style --- B.J. Taylor Brigham Young U. N.G. Roman ADC 1995 Jun 28 If there are comments or questions, please contact: Benjamin J. Taylor taylorb@astro.byu.edu Physics and Astronomy Department, ESC Tel.: 801-378-2233 Brigham Young University FAX: 801-378-2265 Provo, UT 84602 UNKNOWN UNKNOWN The file program.for contains an introduction explaining its use. A few changes to this document have been made by Nancy G. Roman [ADC/SSDOO] V_88.xml Catalogue of ages, metallicities, orbital elements and other parameters for nearby F stars 5089 V/89 Ages, Metallicities, Galactic Orbit of F stars Catalogue of ages, metallicities, orbital elements and other parameters for nearby F stars V A Marsakov Yu G Shevelev Bull. Inf. CDS 47 13 1995 1995BICDS..47...13M Stars, F-type Stars, ages Abundances, [Fe/H] Space velocities Absolute magnitudes, metallicities, effective temperatures, surface gravities, distances, and tangential velocities are calculated for 5498 F stars with homogeneous data on uvby photometry and proper motion, and placed within 80 pc from the Sun. Components of space velocities, eccentricities of galactic orbits, perigalactic and apogalactic distances, and maximal remotness from galactic plane are presented for 1787 stars. Isochrone ages are determined for 3405 slightly evolved stars proceeding from Revised Yale isochrones.
The catalogue HD HD number of the star --- m_HD Component or duplicity indicator --- (b-y)cor Temperature index, corrected for blanketing and luminosity effects (see paper) mag dm1 Colour excess, index of metallicity mag dc1 Colour excess, index of luminosity mag [Fe/H] Metallicity Sun Teff Effective temperature K log.g Gravity cm/s2 MV Absolute magnitude mag Age Age in billion years Gyr GLON Galactic longitude (l) deg GLAT Galactic latitude (b) deg Sp MK spectral classification --- Dist Heliocentric distance pc Vl Tangential velocity in l-direction km/s Vb Tangential velocity in b-direction km/s Uvel Velocity toward Galactic centre km/s Vvel Velocity toward Galactic rotation km/s Wvel Velocity toward Galactic North pole km/s Rp Perigalacticon in kpc kpc Ra Apogalacticon in kpc kpc Zmax Maximal distance from Galactic plane kpc e eccentricity --- paper.tex LaTeX explanations Francois Ochsenbein CDS 1995 Jul 19 V_89.xml A Catalogue of X-Ray Binaries 5090 V/90 Catalogue of X-Ray Binaries A Catalogue of X-Ray Binaries J van Paradijs in 'X-ray Binaries', Lewin W.H.G., van Paradijs J., van den Heuvel E.P.J., Eds., Cambridge University Press, Chapter 14, p. 536-577, ISBN 0 521 41684 1 ??? ??? 1995 1995xrb..book.....L V/82 : Cataclysmic Variables (Ritter) Binaries, X-ray X-ray sources The objects described in this catalog are X-Ray binaries, i.e., semi-detached binary stars in which matter is transferred from a usually more or less normal star to a neutron star or black hole. Thus, cataclysmic variables are not included. The tables provide basic information of the systems as well as selected references. The tables contain 124 low-mass and 69 high mass X-ray binaries.
Ariel-5, CGRO, EXOSAT, GINGA, GRANAT, HEAO-1, HEAO-2, Hakucho, OSO-7, OAO, ROSAT, SAS-3, TENMA, Uhuru, VELA-5, VELA-6
low mass X-ray binaries (LMXB) high mass X-ray binaries (HMXB) ID source name (as hhmm+/-ddd) The source name gives rough information on its B1950 position using the convention hhmm+ddd where hh and mm are the hours and minutes of right ascention, ddd the declanation in units of 0.1 degree. In some cases more or less accurate positions were given. A prefix J indicated that the name was based on J2000 coordinates. --- alt alternate source name --- opt_src1 Opt. counterpart name or location in finding chart Names of optical counterpart, or an asterisk followed by a star number which refers to the star numbers used in the finding chart; the word 'star' refers to a star in the finding chart that has not been given a number or letter. The r_chart column contains the reference to the finding chart. Many optical counterparts have been indicated with a variable-star name, as given in the 'General Catalogue of Variable Stars' (ADC ID's: 2139B, 2172B, 2195) and in recent name lists of variable stars as published in the 'IAU Information Bulletin on Variable Stars', or a number in a well-known catalogue (e.g., HD, SAO). For X-ray sources in globular clusters, the cluster name is given, in addition to the name of a stellar counterpart. --- opt_src2 Opt. counterpart name or location in finding chart --- RAh Right Ascension -hours (B1950) h RAm Right Ascension -minutes min RAs Right Ascension - seconds (accurate to 0.1s) s DE- Declination sign (B1950) --- DEd Declination degrees deg DEm Declination arc minutes arcmin DEs Declination arc seconds (accurate to 1arcsec) arcsec GLON Galactic Longitude (accurate to 0.1 deg) deg GLAT Galactic Latitude deg src_info combination of src_pos and acc_pos, where src_pos = spectral region for positional data acc_pos = positional accuracy indication src_pos: Spectral region that observations were taken for position determination: o: optical x: X-ray r: radio IR: infrared A reference on the source position is given in tab1ref.dat after the key 'pos'. Also included is an indication of the accuracy of that position, in the form of an equivalent (90% confidence level) error radius which can only be considered and approximation (e.g. when the error box is not circular). When no accuracy is quoted it is about one arcsec or better. --- type source type code Codes for source type: A: atoll source (11 LMXBs) [437] B: X-ray burst source (42 LMXBs) D: 'dipping' LMXBs (9) G: globular cluster X-ray source (12 LMXBs) P: X-ray pulsar (3 LMXBs, 29 HMXBs) T: transient X-ray source (41 LMXBs, 30 HMXBs) U: ultrasoft X-ray spectrum (17 LMXBs, 3 HMXBs). These sources include black-hole candidates; some extreme ultra-soft (EUS) source may be white dwarfs on whose surface steady nuclear burning takes place [1184] Z: Z-type (6 LMXBs) --- origin catalogs/experiments listing/detecting source The following codes were used [with reference codes]: A: Ariel V sky survey [795,1255] C: Compton gamma-ray Observatory E: Einstein Observatory Exo: Exosat G: Ginga Gr: Granat H: HEAO 1 A-1 sky survey [1305] Ha: Hakucho K: Kvant M: MIT OSO-7 sky survey [754] OAO: Orbiting Astronomical Observatory R: Rosat S: SAS-3 SL: Space Lab T: Tenma U: Uhuru sky survey [333] V: Vela-5 and -6 satellites. --- LMX_HMXB L = LMXB ; H = HMXB --- r_chart reference code to finding chart --- Vmag visual magnitude optical counterpart mag B-V (B-V) color index optical counterpart mag U-B (U-B) color index optical counterpart mag Other_mag Other magnitude value mag ID_Othr_mag identification of the Other_mag --- Sp Spectral type optical counterpart (HMXB only) --- E(B-V) Estimate for interstellar reddening mag F(X) X-ray flux The flux is given in units of 1 micro Jansky , which is 10**(-29) erg cm**(-2) s**(-1) Hz**(-1) = 2.4 x 10**(-12) erg cm-**(2) s-**(1) keV**(-1) uJy F(X)lo X-ray flux lower limit range uJy F(X)hi X-ray flux upper limit range uJy P Orbital period (unit in unit_P field) --- Ppulse Pulse period for pulsars s unit_P unit of Orbital period --- r_photomtry reference codes for the photometry --- r_F(X) reference codes for the X-ray fluxes --- r_P reference codes for Orbital and Pulse periods --- notes and references to table1.dat notes and references to table2.dat ID Source identification --- note notes to the table for the source --- cross references from often used nomenclature alt Variable star, GX number, Globular Cluster or constellation --- ID Source identification --- table table number --- references refcode code number for reference --- reftext text of reference --- N. Paul Kuin NASA/ADC 1997 Jan 09 UNKNOWN UNKNOWN The catalog was received by the ADC in the form of the original tables. All formatting characters were removed, the notes were placed in a separate file and the data fields were reorganized. The RA and DEC in the tables were reformatted to conform to the same format by expanding decimals where necessary into minutes or seconds. In this process some indication of the positional accuracy has been lost. The tables were checked for consistency with the data format tables. Please report any data that differ from the published tables in any other respects. V_90.xml Radial Velocities of Southern Luminous Stars 5092A V/92A Photometric and Spectroscopic Databases for LSS Stars Radial Velocities of Southern Luminous Stars B C Reed K M Kuhna Astron. Journ. 113 823 1997 1997AJ....113..823R Radial Velocities of Southern Luminous Stars B C Reed Astron. and Astrophys. 117 313 1996 1996A&AS..117..313R Radial Velocities of Southern Luminous Stars B C Reed A E Beatty Astrophys. Journ. Suppl. 97 189 1995 1995ApJS...97..189R Radial Velocities of Southern Luminous Stars B C Reed Astrophys. Journ. Suppl. 87 367 1993 1993ApJS...87..367R III/43 : Luminous Stars in the Southern Milky Way (LSS) (Stephenson+ 1971) Photometry, UBV Photometry, uvby, beta Radial velocities MK spectral classification Stars, luminous Milky Way This catalog contains databases of published photoelectric UBVbeta data, MK-system spectral classifications, and Stroemgren four-color uvby photometry for objects in the Stephenson-Sanduleak "Luminous Stars in the Southern Milky Way" catalog (LSS catalog). The catalog contains mostly OB stars and A and F supergiants. These databases have been compiled from the literature.
UBV and beta photoelectric photometry LSS LSS number --- Flag indicates a remark detailed in notes.dat --- Vmag V band magnitude mag B-V B-V color index mag U-B U-B color index mag o_Vmag Number of UBV observations (measurements) --- beta H-beta mag o_beta Number of H-beta obs. in original reference --- Ncode Note code 1 Emission 2 Double or Spectroscopic Binary or multiple system 3 Variable or suspected variable 4 Subdwarf 5 P Cygni star 6 Wolf-Rayet star 7 See comments in reference cited 8 b uncertain 9 Identification uncertain 10 b quoted to two decimal places only 11 Of star 12 UBV or uvby uncertain 13 Combined result taken from reference cited 14 Crowded field or faint companion(s) 15 Brighter star of a pair with same LSS number quoted in reference cited 16 Radial velocity variable 17 Double-line spectroscopic binary 18 Combined photoelectric/photographic observation 19 Data deriving from CCD observations 20 Carbon star 21 b Cep variable 22 uvby reported to two decimal places only --- r_Vmag Reference on ubvbeta data (file refs.dat) --- MK-system spectral classifications LSS LSS number --- Tclass MK temperature classification --- Lclass MK luminosity class --- Sp Spectral-type qualifiers --- r_Sp Spectroscopic reference code --- DispCode Dispersion code --- N-code Note code, detailed in file codes.dat TG = Transmission grating RG = Reflection grating IT = Image Tube For other codes see codes.dat --- Stroemgren four-color uvby photometry LSS LSS number --- Flag indicates a remark detailed in notes.dat --- b-y b-y color mag m1 m1 is the metallicity index The metallicity index m1 is defined to be (v-b) - (b-y) --- c1 c1 is the Balmer discontinuity index The Balmer discontinuity index c1 is defined to be (u-v) - (v-y) --- o_b-y Number of uvby obs. in original reference --- N-code Note code See the "Note on N-code" section for ubvbeta.dat --- r_b-y Reference code for uvby data (file refs.dat) --- Radial velocity data for each LSS star LSS LSS Number --- note indicates a remark detailed in notes.dat --- HD HD number --- CD CD (Cat. <I/114> designation --- RV Radial velocity km/s e_RV Standard deviation for RV km/s o_RV Number of observations of RV --- Disp Dispersion The format of the majority of the dispersions is: type of instrument used, dispersion in A/mm and the wavelength at which the dispersion applies. These records incorporate a number of abbreviations, as follows: A Angstrom d Hydrogen delta g Hydrogen gamma m/A microns per Angstrom Cass Cassegrain spectrum 1P 1-prism 2P 2-prism 3P 3-prism C Coude spectrum G Grating spectrum (reflection or transmission not specified) IT Image tube spectrum OP Objective-prism P Prism RG Reflection grating S Slit TG Transmission grating TP Thin prism --- Notes Variable type or other note --- Pmag LSS photographic magnitude mag publ Year of publication yr auth First author --- ref Reference --- GLON Galactic longitude deg GLAT Galactic latitude deg name Alternate name of star --- LSS-HD-CPD-CD cross reference LSS LSS (Cat. <III/43>) number --- HD HD (Cat. <III/135>) number --- CPD CPD (Cat. <I/108>) number --- CD CD (Cat. <I/114>) number --- Hbg Heidelberg Objective Prism survey number Catalog by Klare G. and Szeidl B., Veroeff. Heidelberg 18, 9-50 (1966VeHei..18....9K) --- Name Name of object --- GLON Galactic longitude deg GLAT Galactic latitude deg Chart Chart in LSS catalog on which the star appears --- Mag LSS Catalog photographic magnitude mag Notes on individual stars f_LSS / indicates note also refers to this star --- LSS LSS Number --- note Text of note, eventually on several lines --- Codes used for spectroscopy and radial velocity N-code Numerical code --- note Dispersion and comment --- References in numerical order of codes code Numerical code --- --- Period --- note Dispersion and comment --- intro.txt Author's discussion of project and files N.G. Roman ADC/SSDOO 1997 Mar 21 B. Cameron Reed <reed@alma.edu> V_92A.xml A Catalog and Atlas of Cataclysmic Variables - Second Edition 5094 V/94 Catalog and Atlas of Cataclysmic Variables A Catalog and Atlas of Cataclysmic Variables - Second Edition R A Downes R F Webbink M M Shara Publ. Astron. Soc. Pac. 109 345 1997 1997PASP..109..345D V/79 : Catalog and Atlas of Cataclysmic Variables (Downes+ 1993) (Superceded by this catalog). References can be found in the file refs.txt. Atlases Stars, variable This catalog contains data for 1020 cataclysmic variables (CVs). It includes coordinates measured in the reference frame of the Hubble Space Telescope Guide Star Survey for non-novae and from the literature for novae. Also given are the variability type, the magnitude range, references to finding charts and spectroscopy, the galactic latitude and longitude, and the year of outburst for novae. The second edition includes plate identification information for the coordinate measurements, a reference to the classification, proper motion information where appropriate and a table showing the CVs observed by space-based observatories. This version of the catalog includes 195 new objects (172 CVs and 23 non-CVs), revised identifications for 57 objects, and revised classifications and spectral references where available.
A Catalog and Atlas of Cataclysmic Variables - Second Edition as presented here contains a list of all cataclysmic variables discovered prior to May 1996, as derived from the literature; there are a total of 865 cataclysmic variables (276 novae, 372 dwarf novae, 162 novalike variables, 47 objects classified only as cataclysmic variables, 6 interacting binary white dwarf (IBWD), and 2 possible supernovae/novae) and 155 object formerly classified as cataclysmic variables. A Catalog and Atlas of Cataclysmic Variables - Second Edition as distributed here is in two files. The first file contains the cataclysmic variables in constellation order, while the second contains the objects in order of increasing right ascension. The tables below give the characteristics of these files. A copy of the document catvar.tex should be transmitted with any additional copy of this catalog.
Sorted by Constellation Sorted by Right Ascension GCVS GCVS name The name of the object in the General Catalogue of Variable Stars and subsequent Namelists (67th, Kholopov et al. 1985; 68th, Kholopov et al. 1987; 69th, Kholopov et al. 1989; 70th, Kazarovets and Samus 1990; 71st, Kazarovets, Samus, and Goranskij 1993; 72nd, Kazarovets and Samus 1995). For those objects without variable star designations (189), we list the constellation name only (which were derived from Roman [1987]). Since some constellations contain more than one object without a GCVS designation, we include a number after the constellation name. The non-GCVS designations are strictly provisional. --- RAh Right ascension (J2000) h RAm Right ascension minutes (J2000) min RAs Right ascension seconds (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination minutes (J2000) arcmin DEs Declination seconds (J2000) When the seconds of declination were not known, this field has been left blank. arcsec GLAT Galactic latitude deg var_type Classification --- nova_yr Year of outburst (novae) yr --- indicating less than --- max_mag Maximum brightness MAG. RANGE: The MAXimum and MINimum magnitudes for the objects. For novae the primary source is Duerbeck (1987a), while for the non-novae the catalog of Ritter (1990) is the prime source. When no other references to brightness were available, the GCVS values were used. mag u_max_mag indicating uncertainty --- sys_max System for maximum mag. MAG. SYSTEM: See Table 4. Table 4: Magnitude Abbreviations Magnitude Definition _________ _________________________ U Johnson U B Johnson B V Johnson V I Johnson I f m2200 v visual p photographic r red j SRC j (unfiltered IIIa-J) --- --- extra character --- --- indicating greater than --- min_mag Minimum brightness mag u_min_mag indicating uncertainty --- sys_min System for minimum mag. --- r_RAh Coordinate reference COORD REF: A code for a reference to the coordinates. Entries with a four-character code correspond to plate-IDs from the Hubble Space Telescope Guide Star survey; other codes refer to references in file coordrefs.dat. An asterisk (*) following the references means that there is a comment regarding the coordinate measurement, and those Downes and Shara (1993) references which have been superseded are listed as "deleted". --- --- Comment flag --- type_ref Classification reference CLASSIFICATION REF: A code for a reference to the CV classification. The file typerefs.dat defines the codes from the literature. An asterisk (*) following the references means that there is a comment regarding the classification. --- --- Comment flag --- chart Chart reference CHART REF: for those objects with charts presented in the source referenced (168 objects) or in Downes and Shara (1993), a code for the original reference from which our chart is based. Note that the identifications of the CVs are based on the published charts (or in some cases coordinates only), and have not been independently verified by the authors. The file chartrefs.dat defines the codes and includes the numeric code used in the GCVS and subsequent Namelists. For novae (276 objects) a reference to the previously published chart in Duerbeck (1987a) is given (except for recent novae). An asterisk(*) following the references means that there is a comment regarding the identification, and those Downes and Shara (1993) references which have been superseded are listed as "deleted". The letter following some GVCS numbers in chartrefs.dat indicates the source of the identification as follows: a from Kholopov, Samus, Kazarovets, and Perova 1985 b from Kholopov, Samus, Kazarovets, and Kireeva 1987 c from Kholopov, Samus, Kazarovets, Frolov, and Kireeva 1989 d from Kazarovets and Samus 1995 --- n_chart Comment flag --- spect Spectrum reference SPEC REF: A code for a reference to a published spectrum; file spectrefs.dat defines the codes. A prefix of S indicates a spectrum in quiescence (394 objects), while a prefix of X indicates a spectrum in outburst (121 objects); we were unable to locate spectra for 350 objects. Whenever available, the quiescent spectrum was chosen for the catalog over an outburst spectrum. A colon (:) following the reference indicates that (i) the spectrum is only described, (ii) the spectrum is a glass plate tracing, or (iii) the reference is unconfirmed (only for a few novae in Duerbeck 1987a), and those Downes and Shara (1993) references which have been superseded are listed as "deleted". --- n_spect Comment flag --- ID Other name OTHER NAME: A discovery or common alternative (non-GCVS) designation for the object. --- Table 7: Chart references code Code for chart reference --- GCVS GCVS number --- ref References text a From Kholopov, Samus, Kazarovets, and Perova 1985. b From Kholopov, Samus, Kazarovets, and Kireeva 1987. c From Kholopov, Samus, Kazarovets, Frolov, and Kireeva. 1989 --- Table 5: Coordinate references code Code for coordinate reference --- ref References text --- Table 8: Spectrum references prefix Quiescent/outburst spectrum --- code Code for spectrum reference --- ref References text --- Table 6: Type references code Code for type reference --- ref References text --- References ref References text --- catvar.tex LaTeX Document refs.txt References J. E. Gass ADC/SSDOO 1997 Mar 11 UNKNOWN UNKNOWN The original document (Documentation for the Computer-Readable Version by Ronald A. Downes, Doc. No. NSSDC/WDC-A-R&S 97-?? (??? 1997) was reformatted according to the CDS documentation standard. V_94.xml Preliminary Fourth Edition of the Catalogue on Variable Stars in Globular Clusters 5097 V/97 Updated 3rd Cat Variable Stars in Globular Clusters Preliminary Fourth Edition of the Catalogue on Variable Stars in Globular Clusters C Clement unpublished ??? ??? 1997 1997 Preliminary Fourth Edition of the Catalogue on Variable Stars in Globular Clusters H Sawyer Hogg Publications of the David Dunlap Observatory, University of Toronto, Vol 3, No 6 ??? ??? 1973 1973PDDO....3....6S http://lepus.astro.utoronto.ca/ : (???) Stars, variable Clusters, globular This Catalogue is an update to Helen Sawyer Hogg's Third Catalogue on Variable Stars in Globular Clusters (1973, David Dunlap Observatory Publications, Volume 3, Number 6). This update is based mainly on reference cards prepared by Helen Sawyer Hogg from articles published in the literature in the period 1973 to 1988. There are also some references entered from more recent literature and we are attempting to bring the catalogue up to date. Not all known globular clusters have been included, as the literature search is not at this point complete.
Globular Cluster data clusterID IAU name The name of the file indicates the IAU cluster name, in the format C####p### or C####m###, where the "p" and "m" indicate plus or minus, as there may be difficulty in naming files with "-" or "+" on host systems. --- RAh Right Ascension hours h RAm RA minutes min DE- Declination sign --- DEd Declination degrees deg DEm Declination arc minutes arcmin Epoch =1950.0 epoch of coordinates if not 1950 There is some uncertainty about the reliability of the epoch values. Use them with caution. A future update will resolve this issue. yr name cluster name and other designations --- cluster_ID IAU name with +/- sign for p/m --- Nvar number of variables or any known variables in or around the cluster --- Variables in and near Globular Clusters clusterID Cluster's IAU name --- var var #, or other id --- X pos x (north) relative to center arcsec Y pos y (east) of the cluster arcsec u_Y uncertainty in Y --- l_max_mag limits to maximum magnitude (usually V or B) --- max_mag maximum magnitude (unless noted otherwise) mag u_max_mag uncertainty flags --- l_min_mag upper limit minimum magnitude --- min_mag minimum magnitude (unless noted otherwise) mag u_min_mag uncertainty flags --- epoch Epoch(max mag) --- u_epoch uncertainty flags --- l_P upper limit period P --- P Period (in seconds) for long periods see the remarks s u_P uncertain period flag (#=::) --- remarks pointers to references, names from objects by authors, variablility, membership, alternate periods In the remarks the following abbreviations are used: + or - : increasing or decreasing period var: variable not var: determined not to be variable mem: member of the cluster f: field star note (1): The visual magnutude data were originally given in mean V and amplitude but were converted to fit in the table. See the original data file on the object. note (2): Epoch is the time of maximum for RR Lyrae and XX PHe and minimum for the EW variables. note(3): Not the maximum and minimum visual amplitudes, but mean(B) and amplitude are given. --- References to the data ID IAU name cluster --- text reference and notes pertaining to the reference A few new abbreviations are used here in regard to the literature consulted. They include: A&SS - Astrophysics and Space Science CA&A - Chinese Astronomy and Astrophysics CA - Chinese Astronomy SA - Soviet Astronomy SA Lett - Soviet Astronomy Letters --- Remarks and notes ID IAU name cluster --- note notes to the variabls.dat table --- byclustr.txt Data Organized by Cluster This data file is the original data from the author, and organized by cluster. The file format is first some information about the cluster (which has been put in table clusters.dat), then the table of the variables' properties (see the table variabls.dat), followed by notes about the data (see notes.dat) and references (see references.dat). The extracted tabular data hopefuly will make searches easier to do. Please note that not all known globular clusters have been included, as the literature search is not at this point complete. At the beginnning of the file is a header containing the cluster name, with multiple designations shown if they are in common use. Following are the RA and Dec of the cluster. The RA and Dec are the 1950 coordinates unless otherwise noted. This is followed by a listing of any known variables in or around the cluster. This section will be discussed in more detail elsewhere. Following the variable star listing is a bibliographical listing of papers related to the cluster. Brief notes accompany each reference to aid in locating the information desired. The bibliographical references are sorted approximately chronologically. Due to space limitations the summary notes are very brief and should only be taken as an indication of the nature of the article. It should be noted that the references from approximately 1973 to 1988 are fairly complete and are based on reference cards prepared by Helen Sawyer Hogg. The literature survey is ongoing. For references dating back earlier than 1973, one should refer to the 3rd Catalogue of Variable Stars in Globular Clusters (Sawyer Hogg, 1973) and the references contained therein. N.P.M. Kuin ADC 1997 Oct 29 Author's Contact Information: Any questions or queries should be addressed to Christine Clement at cclement@astro.utoronto.ca who is maintaining the catalogue. UNKNOWN UNKNOWN The catalog was submitted to the ADC by Christine Clement. The update for 1973 to 1988 was prepared by Tara Rosebery and Quentin Dufton under the supervision of Christine Clement. A further update has been prepared by Jay Burford. The catalog was received by the ADC 16-Apr-1997 in the format closely matching that of Sawyer Hogg's 3rd Catalogue of Variable Stars in Globular Clusters. The data were extensively reorganized by P. Kuin to provide several tables of the basic information in addition to the data given for each cluster in one single file. The identifyer for each Globular Cluster was added to the new tables. V_97.xml The MSX Infrared Astrometric Catalog 5098 V/98 MSX Infrared Catalog The MSX Infrared Astrometric Catalog M P Egan S D Price Astron. J 112 2862 1996 1996AJ....112.2862E II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) II/126 : IRAS Serendipitous Survey Catalog (Kleinmann+ 1986) II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989) II/209 : Catalog of Infrared observations, Edition 3.5 (Gezari+ 1996) http://www.ipac.caltech.edu/ipac/msx/msx.html : MSX page http://www.sdl.usu.edu/programs/spirit3/spirit3.html : SPIRIT III page Infrared sources Proper motions Spectroscopy Cross identifications This version of the MSX IR Astrometric Catalog is a truncated version of the documentation which exists for the convenience of the user and is primarily intended to allow quick access to the file formats and other information needed to access the information. The AJ paper contains the definitive information about the catalog itself. The MSX IR Astrometric Catalog, Version 4.2.1 was constructed from a number of visible astrometric catalogs, and contains position information accurate to the sub-arcsecond level. The FK5 (1988 Fricke Schwan & Lederle, Cat. <I/149>), FK5 Extension (1991 Fricke, Schwan & Corbin, Cat. <I/175>), Astrographic Catalog of Reference Stars (1991 Corbin & Urban, Cat. <I/171>), Position and Proper Motion Catalog (1988 Roeser & Bastian, Cat. <I/146>) and PPM South (1991 Bastian et al., Cat. <I/193>) were the sources of position and magnitude information. The PPM and FK5 catalogs contain 1-D spectral type information, and this was supplemented where possible with 2-D MK spectral types. The ACRS and PPM quote photographic magnitudes. These were transformed to V magnitude using the spectral type and expected B-V color. Spatial coincidence and color-matching criteria (based on V-[12] color and spectral type) were used to identify IR counterparts of the astrometric stars. The IRAS Point Source (Cat. <II/125>), Faint Source (Cat. <II/156>), Faint Source Reject file, and Serendipitous Survey (Cat. <II/126>) catalogs were used to supply IR observations, as was the Catalog of Infrared Observations (1993 Gezari et al., Cat <II/209>). The infrared telescope (SPIRIT III) aboard the Ballistic Missile Defense Organization (BMDO) Midcourse Space Experiment (MSX) (Mill et al., 1994, J. of Spacecraft & Rockets 31, 900) has detectors which allow spatial resolution 30 times better than that achieved by IRAS The IR flux in each SPIRIT III band was estimated using the V magnitude, spectral type, and IR flux (if available) to determine a blackbody spectrum for the star, which was then convolved with the system spectral response of each SPIRIT III radiometer band. Stars which were brighter than 8th magnitude in band A were retained in the final MSX IR astrometric catalog. In MSXv4.2.1, there are 177860 stars, 61242 of which had IR counterparts. The MSX Infrared Astrometric Catalog has been contructed as a tool for improving the pointing accuracy of infrared observations. The catalog contains 177,860 astrometric stars, 61,242 which have been identified with their infrared counterparts from IRAS catalogs and the Catalog of Infrared Observations through position and color matching. Infrared flux densities are predicted for 6 wavelength bands between 4 and 22um. The catalog identifications are complete to within the spatial coverage of current surveys for those astrometric stars brightest in the infrared. By predicting fluxes of astrometric stars without IR identifications we are able to extend the catalog to areas of the sky which were incomplete in the IRAS catalogs. Furthermore, by retaining stars below the brightness limit of current surveys we are able to provide better spatial coverage to help point or position the next generation of infrared telescopes.
MSX Infrared Astrometric Catalog AsID Original astrometric catalog ID F FK5, Cat. <I/149> f FK5 Extension, Cat. <I/175> A ACRS, Cat. <I/171> N PPM, Cat. <I/146> S PPM South, Cat. <I/193> --- AsName Astrometric catalog number --- IrID IR catalog ID P IRAS Point Source Catalog, Cat. <II/125> F IRAS Faint Source Catalog, Cat. <II/156> B Combined PSC/FSC data, Cat. <II/125> and Cat. <II/156> Z IRAS Faint Source Reject S IRAS Serendiptious Survey, Cat. <II/126> C Catalog of IR Observations, Cat. <II/209> --- IrName Name of star in IR catalog --- RAh Right ascension, J2000 h RAm Right ascension, J2000 min RAs Right ascension, J2000 s DE- Sign of declination --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec e_RAs Mean R.A. error*cos(dec) ms e_DEs Mean declination error 0.01arcsec pmRA Proper motion in right ascension (J2000) 10-2s/yr pmDE Proper motion in declination (J2000) 10-2arcsec/yr e_pmRA Mean error of R.A. PM*cos(dec) 0.1mas/yr e_pmDE Mean error of Dec. PM 0.1mas/yr Sp Spectral type Coded spectral type, e.g. G83 = G8 III; G80 = G8 --- LRS IRAS LRS designation --- Vmag V visual magnitude mag F12um E+00 IRAS 12mu flux Jy F25um E+00 IRAS 25mu flux Jy F60um E+00 IRAS 60mu flux Jy F100um E+00 IRAS 100mu flux Jy q_F12um IRAS 12um flux quality flag --- q_F25um IRAS 25um flux quality flag --- q_F60um IRAS 60um flux quality flag --- q_F100um IRAS 100um flux quality flag --- FSIIIA SPIRIT III Band A flux density estimate Jy FSIIIB1 SPIRIT III Band B1 flux density estimate Jy FSIIIB2 SPIRIT III Band B2 flux density estimate Jy FSIIIC SPIRIT III Band C flux density estimate Jy FSIIID SPIRIT III Band D flux density estimate Jy FSIIIE SPIRIT III Band E flux density estimate Jy F12umEst Estimated IRAS 12 micron flux Jy Lam1 Wavelength of CIO observation These values were originally embedded in the IRAS Fxxum columns. um Flux1 Corresponding Flux of CIO observation Jy Lam2 Wavelength of CIO observation um Flux2 Corresponding Flux of CIO observation Jy Francois Ochsenbein CDS 1997 Dec 04 UNKNOWN UNKNOWN * 06-Nov-1996: AAS CD-ROM series, Volume 7, 1996, Lee Brotzman [ADS] * 04-Dec-1997: Wavelength + fluxes from CIO disentangled from IRAS fluxes V_98.xml Catalogue of cataclysmic binaries, low-mass X-ray binaries and related objects (6th Edition) 5099 V/99 Cataclysmic Binaries and LMXB Catalogue Catalogue of cataclysmic binaries, low-mass X-ray binaries and related objects (6th Edition) H Ritter U Kolb Astron. Astrophys. Suppl. Ser. 129 83 1998 1998A&AS..129...83R Binaries, cataclysmic Binaries, X-ray Novae catalogs novae, cataclysmic variables binaries: close X-rays: stars Cataclysmic Binaries are semi-detached binaries consisting of a white dwarf or a white dwarf precursor primary and a low-mass secondary which is filling its critical Roche lobe. The secondary is not necessarily unevolved, it may even be a highly evolved star as for example in the case of the AM CVn-type stars. Low-Mass X-Ray Binaries are semi-detached binaries consisting of either a neutron star or a black hole primary, and a low-mass secondary which is filling its critical Roche lobe. Related Objects are detached binaries consisting of either a white dwarf or a white dwarf precursor primary and of a low-mass secondary. The secondary may also be a highly evolved star. The catalogue lists coordinates, apparent magnitudes, orbital parameters, stellar parameters of the components and other characteristic properties of 318 cataclysmic binaries, 47 low-mass X-ray binaries and 49 related objects with known or suspected orbital periods together with a comprehensive selection of the relevant recent literature. In addition the catalogue contains a list of references to published finding charts for 394 of the 414 objects. A cross-reference list of alias object designations concludes the catalogue. Literature published before 30 June 1997 has, as far as possible, been taken into account. This catalogue supersedes the 5th edition (catalogue <V/59>) and the updated list by Ritter and Kolb (1995; catalogue <V/82>).
Catalogue of Cataclysmic Binaries Name Object name number=1 Wherever possible, the designation of the object given in the General Catalogue of Variable Stars (Cat. <II/139>) is used here. --- whoswho * indicating that further alternative designations are in the whoswho*.dat files --- Alt_Name A frequently used alternative name --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes of arc) arcmin DEs Declination J2000 (seconds of arc) arcsec epos Accuracy of position in hexadecimal number=2 Accuracy written in hexadecimal: A=10", B=11", C=12", D=13", E=14", F=15". If the positional error is larger than 15arcsec, this field is blank arcsec Type1 Object type number=3 Object type coarsely characterised using the following abbreviations: AC = AM CVn star, spectrum devoid of hydrogen lines, subtype of NL AM = polar = AM Her system, subtype of NL, contains a synchronously rotating, magnetized white dwarf AS = subtype of AM, with a slowly asynchronously rotating, magnetized white dwarf CP = coherent pulsator, contains a coherently pulsating white dwarf DD = system consists of two degenerate components DN = dwarf nova DQ = DQ Her star, contains a non-synchronously rotating, magnetized white dwarf; usually not seen in X-rays ER = ER UMa star = SU UMa star with an extremely short supercycle IP = intermediate polar, shows coherent X-ray period from a non-synchronously spinning, magnetized white dwarf; usually a strong X-ray source N = classical nova Na = fast nova (decline from max. by 3mag in less than about 100days) Nb = slow nova (decline from max. by 3mag in more than about 100days) Nc = extremely slow nova (typical time scale of the decline from maximum: decades) NL = nova-like variable Nr = recurrent nova SH = non-SU UMa star showing either permanent or transient superhumps SS = supersoft X-ray source; CV with stationary hydrogen burning on the white dwarf SU = SU UMa star, subtype of DN SW = SW Sex star, subtype of NL UG = dwarf nova of either U Gem or SS Cyg subtype UX = UX UMa star, subtype of NL VY = VY Scl star (anti dwarf nova), subtype of NL WZ = WZ Sge star = SU UMa star with an extremely long supercycle ZC = Z Cam star, subtype of DN --- u_Type1 Uncertainty flag for object type --- Type2 Object type number=3 Object type coarsely characterised using the following abbreviations: AC = AM CVn star, spectrum devoid of hydrogen lines, subtype of NL AM = polar = AM Her system, subtype of NL, contains a synchronously rotating, magnetized white dwarf AS = subtype of AM, with a slowly asynchronously rotating, magnetized white dwarf CP = coherent pulsator, contains a coherently pulsating white dwarf DD = system consists of two degenerate components DN = dwarf nova DQ = DQ Her star, contains a non-synchronously rotating, magnetized white dwarf; usually not seen in X-rays ER = ER UMa star = SU UMa star with an extremely short supercycle IP = intermediate polar, shows coherent X-ray period from a non-synchronously spinning, magnetized white dwarf; usually a strong X-ray source N = classical nova Na = fast nova (decline from max. by 3mag in less than about 100days) Nb = slow nova (decline from max. by 3mag in more than about 100days) Nc = extremely slow nova (typical time scale of the decline from maximum: decades) NL = nova-like variable Nr = recurrent nova SH = non-SU UMa star showing either permanent or transient superhumps SS = supersoft X-ray source; CV with stationary hydrogen burning on the white dwarf SU = SU UMa star, subtype of DN SW = SW Sex star, subtype of NL UG = dwarf nova of either U Gem or SS Cyg subtype UX = UX UMa star, subtype of NL VY = VY Scl star (anti dwarf nova), subtype of NL WZ = WZ Sge star = SU UMa star with an extremely long supercycle ZC = Z Cam star, subtype of DN --- u_Type2 Uncertainty flag for object type --- Type3 Object type number=3 Object type coarsely characterised using the following abbreviations: AC = AM CVn star, spectrum devoid of hydrogen lines, subtype of NL AM = polar = AM Her system, subtype of NL, contains a synchronously rotating, magnetized white dwarf AS = subtype of AM, with a slowly asynchronously rotating, magnetized white dwarf CP = coherent pulsator, contains a coherently pulsating white dwarf DD = system consists of two degenerate components DN = dwarf nova DQ = DQ Her star, contains a non-synchronously rotating, magnetized white dwarf; usually not seen in X-rays ER = ER UMa star = SU UMa star with an extremely short supercycle IP = intermediate polar, shows coherent X-ray period from a non-synchronously spinning, magnetized white dwarf; usually a strong X-ray source N = classical nova Na = fast nova (decline from max. by 3mag in less than about 100days) Nb = slow nova (decline from max. by 3mag in more than about 100days) Nc = extremely slow nova (typical time scale of the decline from maximum: decades) NL = nova-like variable Nr = recurrent nova SH = non-SU UMa star showing either permanent or transient superhumps SS = supersoft X-ray source; CV with stationary hydrogen burning on the white dwarf SU = SU UMa star, subtype of DN SW = SW Sex star, subtype of NL UG = dwarf nova of either U Gem or SS Cyg subtype UX = UX UMa star, subtype of NL VY = VY Scl star (anti dwarf nova), subtype of NL WZ = WZ Sge star = SU UMa star with an extremely long supercycle ZC = Z Cam star, subtype of DN --- u_Type3 Uncertainty flag for Object type --- Type4 Object type number=3 Object type coarsely characterised using the following abbreviations: AC = AM CVn star, spectrum devoid of hydrogen lines, subtype of NL AM = polar = AM Her system, subtype of NL, contains a synchronously rotating, magnetized white dwarf AS = subtype of AM, with a slowly asynchronously rotating, magnetized white dwarf CP = coherent pulsator, contains a coherently pulsating white dwarf DD = system consists of two degenerate components DN = dwarf nova DQ = DQ Her star, contains a non-synchronously rotating, magnetized white dwarf; usually not seen in X-rays ER = ER UMa star = SU UMa star with an extremely short supercycle IP = intermediate polar, shows coherent X-ray period from a non-synchronously spinning, magnetized white dwarf; usually a strong X-ray source N = classical nova Na = fast nova (decline from max. by 3mag in less than about 100days) Nb = slow nova (decline from max. by 3mag in more than about 100days) Nc = extremely slow nova (typical time scale of the decline from maximum: decades) NL = nova-like variable Nr = recurrent nova SH = non-SU UMa star showing either permanent or transient superhumps SS = supersoft X-ray source; CV with stationary hydrogen burning on the white dwarf SU = SU UMa star, subtype of DN SW = SW Sex star, subtype of NL UG = dwarf nova of either U Gem or SS Cyg subtype UX = UX UMa star, subtype of NL VY = VY Scl star (anti dwarf nova), subtype of NL WZ = WZ Sge star = SU UMa star with an extremely long supercycle ZC = Z Cam star, subtype of DN --- u_Type4 Uncertainty flag for Object type --- l_mag1 Limit flag for magnitude mag1 --- mag1 Apparent V (B) magnitude at maximum brightness number=4 Apparent V magnitude at maximum brightness of: novae (N,Na,Nb,Nc,Nr) in minimum DN (UG,ZC,SU) in minimum NL (UX,AC) in normal state NL (AM,VY) in high state. mag f_mag1 ":?" uncertainty flag on mag1 "B" if mag1 is the apparent B magnitude --- l_mag2 Limit flag for magnitude mag2 --- mag2 Apparent V (B) magnitude at maximum brightness number=5 In case of eclipses magnitude at mideclipse, of: novae (N,Na,Nb,Nc,Nr) in minimum DN (UG,ZC,SU) in minimum NL (UX,AC) in normal state NL (AM,VY) in high state. mag f_mag2 ":?" uncertainty flag on mag2 "B" if mag2 is the apparent B magnitude --- l_mag3 Limit flag for magnitude mag3 --- mag3 Apparent V (B) magnitude at maximum brightness number=6 Apparent magnitude at maximum brightness of: novae (N,Na,Nb,Nc,Nr) in outburst DN (UG,ZC) in outburst DN (SU) in normal outburst NL (AM,VY) in low state NL (DQ,IP) in flaring state. mag f_mag3 ":?" uncertainty flag on mag3 "B" if mag3 is the apparent B magnitude --- l_mag4 Limit flag for magnitude mag4 --- mag4 Apparent V (B) magnitude number=7 Apparent magnitude of ZC in standstill, SU in superoutburst, at minimum brightness of NL (AM,VY), in low state. mag f_mag4 ":?" uncertainty flag on mag4 "B" if mag4 is the apparent B magnitude --- T1 Time interval between two subsequent outbursts number=8 Time interval between outbursts is defined: - for dwarf novae of subtype UG or ZC: the typical time interval between two subsequent outbursts; - for dwarf novae of subtype SU: T1 is the typical time interval between two subsequent normal outburst, and T2 is the typical time interval between subsequent superoutbursts. d T2 Time interval between two subsequent outbursts number=8 Time interval between outbursts is defined: - for dwarf novae of subtype UG or ZC: the typical time interval between two subsequent outbursts; - for dwarf novae of subtype SU: T1 is the typical time interval between two subsequent normal outburst, and T2 is the typical time interval between subsequent superoutbursts. d Orb.Per Orbital period, in case of object type DQ: spectroscopic period, if it is different from the photometric one d u_Orb.Per Uncertainty flag for Orb.Per number=9 the * indicates, in case of object type SU, that the orbital period has been estimated from the known superhump period using the empirical relation given by B. Stolz and R. Schoembs (1984A&A...132..187S). --- 2.__Per Second period number=10 The second period is, in case of object type: DQ or IP: photometric period if it is different from the spectroscopic one AM: polarization period = spin period of the white dwarf, if it is different from the presumed orbital period (subtype AS) SU: superhump period, wherever possible, at the beginning of a superoutburst SH: photometric period, presumably superhump period of either permanent or transient superhumps d u_2.__Per Uncertainty flag for 2.__Per --- 3.__Per Additional period in the system number=11 This additional period is, in case of object type: CP: period of coherent pulsation, (transient if f_3.__Per=T) DQ: spin period of the white dwarf IP: spin period of the white dwarf, usually detected in X-Rays s f_3.__Per Flag for 3.__Per number=12 the flag takes the values: ':' uncertainty flag 'T' indicating transient pulsations 'Q' indicating the occurrence of quasi- periodic oscillations (QPO) in objects of type N, DN, NL. --- 4.__Per Additional period in the system number=13 This additional period is, in case of object type: CP: second period of coherent pulsation, (transient if f_4.__Per=T) DQ: additional period, presumably due to reprocessed X-Rays IP: additional period, usually seen in the optical and presumably due to reprocessed X-Rays s f_4.__Per ":" uncertainty flag for 4.__Per "T" flag indicating transient pulsations --- EB Flag indicating the occurrence of eclipses number=14 The EB flag means: EB= : (blank) no eclipses observed. EB=1: 1 eclipse per orbital revolution observed. EB=2: 2 eclipses per orbital revolution observed. EB=D: periodic eclipse-like dips observed. --- SB Flag specifying the type of spectroscopic binary number=15 The SB flag means: SB=1: single-line spectroscopic binary SB=2: double-line spectroscopic binary --- SpType2 Spectral type of the secondary number=16 Spectral types are given in the following format: [Spectral class/Luminosity class], where the usual roman numerals for the latter are replaced by the corresponding arabic numerals, i.e. I = 1, II = 2, III = 3, IV = 4, V = 5, VI = 6. --- SpType1 Spectral type of the primary number=16 Spectral types are given in the following format: [Spectral class/Luminosity class], where the usual roman numerals for the latter are replaced by the corresponding arabic numerals, i.e. I = 1, II = 2, III = 3, IV = 4, V = 5, VI = 6. --- l_M1/M2 Limit flag for M1/M2 --- M1/M2 Mass ratio M1/M2 --- u_M1/M2 Uncertainty flag for M1/M2 --- e_M1/M2 Error of M1/M2 --- l_Incl Limit flag for the orbital inclination --- Incl Orbital inclination deg u_Incl Uncertainty flag for the inclination --- e_Incl Error of orbital inclination deg l_M1 Limit flag for primary mass M1 --- M1 Primary mass M1 solMass u_M1 Uncertainty flag for primary mass M1 --- e_M1 Error of primary mass M1 solMass l_M2 Limit flag for secondary mass M2 --- M2 Secondary mass M2 solMass u_M2 Uncertainty flag for secondary mass M2 --- e_M2 Error of secondary mass M2 solMass Catalogue of Low-Mass X-Ray Binaries Name Object name number=1 Wherever possible, the designation of the object given in the General Catalogue of Variable Stars (Cat. <II/139>) is used here --- whoswho * indicating that further alternative designations are in the whoswho?dat files --- Alt_Name A frequently used alternative name --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes of arc) arcmin DEs Declination J2000 (seconds of arc) arcsec epos Accuracy of position in hexadecimal number=2 Accuracy written in hexadecimal: A=10", B=11", C=12", D=13", E=14", F=15" If the positional error is larger than 15arcsec, this field is blank arcsec Type1 Object type number=3 the object type is coarsely characterised using the following abbreviations: AS = atoll source, subtype of the LMXBs BH = black hole candidate, subtype of the LMXBs DC = source with an accretion disc corona, subtype of the LMXBs GC = source in a globular cluster SH = system showing either permanent or transient superhumps XB = X-ray burst source XP = X-ray pulsar XT = transient X-ray source ZS = Z-source, subtype of the LMXBs --- u_Type1 Uncertainty flag for object type --- Type2 Object type number=3 the object type is coarsely characterised using the following abbreviations: AS = atoll source, subtype of the LMXBs BH = black hole candidate, subtype of the LMXBs DC = source with an accretion disc corona, subtype of the LMXBs GC = source in a globular cluster SH = system showing either permanent or transient superhumps XB = X-ray burst source XP = X-ray pulsar XT = transient X-ray source ZS = Z-source, subtype of the LMXBs --- u_Type2 Uncertainty flag for object type --- Type3 Object type number=3 the object type is coarsely characterised using the following abbreviations: AS = atoll source, subtype of the LMXBs BH = black hole candidate, subtype of the LMXBs DC = source with an accretion disc corona, subtype of the LMXBs GC = source in a globular cluster SH = system showing either permanent or transient superhumps XB = X-ray burst source XP = X-ray pulsar XT = transient X-ray source ZS = Z-source, subtype of the LMXBs --- u_Type3 Uncertainty flag for Object type --- Type4 Object type number=3 the object type is coarsely characterised using the following abbreviations: AS = atoll source, subtype of the LMXBs BH = black hole candidate, subtype of the LMXBs DC = source with an accretion disc corona, subtype of the LMXBs GC = source in a globular cluster SH = system showing either permanent or transient superhumps XB = X-ray burst source XP = X-ray pulsar XT = transient X-ray source ZS = Z-source, subtype of the LMXBs --- u_Type4 Uncertainty flag for Object type --- l_mag1 Limit flag for magnitude mag1 --- mag1 Apparent V (B) magnitude at maximum brightness, in case of XT in quiescence mag f_mag1 ":" uncertainty flag "B" if mag1 is the apparent B magnitude --- l_mag2 Limit flag for magnitude mag2 --- mag2 Apparent V (B) magnitude at minimum brightness number=4 in case of eclipses magnitude at mideclipse, in case of XT in quiescence mag f_mag2 "B" if mag2 is the apparent B magnitude --- mag3 Apparent V (B) magnitude at maximum brightness number=5 in case of XL (XB, XT) in outburst mag u_mag3 Uncertainty flag for magnitude mag3 --- mag4 Apparent V (B) magnitude mag l_LX/Lopt Limit flag on LX/Lopt --- LX/Lopt The ratio of X-ray to optical luminosity --- T1 Typical time interval between two subsequent X-ray active states in case of subtype XT d Orb.Per Orbital period d u_Orb.Per Uncertainty flag for Orb.Per --- 2.__Per Second period, in case of object type SH: photometric period, presumably superhump period of either permanent or transient superhumps d u_2.__Per Uncertainty flag for 2.__Per --- 3.__Per Additional period in the system, in case of object type XP: pulse period of the pulsar s f_3.__Per Flag for 3.__Per number=6 the flag means: ':' uncertainty flag 'T' transient pulsations 'Q' occurrence of quasi-periodic oscillations (QPO) in objects of type N, DN, NL --- 4.__Per Aditional period in the system, in case of object type XP: optical period, presumably due to e_processed X-Rays s f_4.__Per Note on 4.__Per number=6 the flag means: ':' uncertainty flag 'T' transient pulsations 'Q' occurrence of quasi-periodic oscillations (QPO) in objects of type N, DN, NL --- EB Occurrence of eclipses number=7 The EB flag means: EB= : (blank) no eclipses observed. EB=1: 1 eclipse per orbital revolution observed. EB=2: 2 eclipses per orbital revolution observed. EB=D: periodic eclipse-like dips observed. --- SB Flag specifying the type of spectroscopic binary number=8 The SB flag means: SB=1: single-line spectroscopic binary SB=2: double-line spectroscopic binary --- SpType2 Spectral type of the secondary number=9 Spectral types are given in the following format: [Spectral class/Luminosity class], where the usual roman numerals for the latter are replaced by the corresponding arabic numerals, i.e. I = 1, II = 2, III = 3, IV = 4, V = 5, VI = 6. --- SpType1 Spectral type of the primary number=9 Spectral types are given in the following format: [Spectral class/Luminosity class], where the usual roman numerals for the latter are replaced by the corresponding arabic numerals, i.e. I = 1, II = 2, III = 3, IV = 4, V = 5, VI = 6. --- l_M1/M2 Limit flag for M1/M2 --- M1/M2 Mass ratio M1/M2 --- u_M1/M2 Uncertainty flag for M1/M2 --- e_M1/M2 Error of M1/M2 --- l_Incl Limit flag for the orbital inclination --- Incl Orbital inclination deg u_Incl Uncertainty flag for the inclination --- e_Incl Error of orbital inclination deg M1 Primary mass M1 solMass u_M1 Uncertainty flag for primary mass M1 --- e_M1 Error of primary mass M1 solMass l_M2 Limit flag for secondary mass M2 --- M2 Secondary mass M2 solMass u_M2 Uncertainty flag for secondary mass M2 --- e_M2 Error of secondary mass M2 solMass Catalogue of Related Objects Name Object name number=1 Wherever possible, the designation of the object given in the General Catalogue of Variable Stars (Cat. <II/139>) is used here. --- whoswho * indicating that further alternative designations are in the whoswho*.dat files --- Alt_Name A frequently used alternative name --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes of arc) arcmin DEs Declination J2000 (seconds of arc) arcsec epos Accuracy of position in hexadecimal number=2 Accuracy written in hexadecimal: A=10", B=11", C=12", D=13", E=14", F=15". If the positional error is larger than 15arcsec, this field is blank arcsec Type1 Object type number=3 Object type coarsely characterised using the following abbreviations: DD = system consists of two degenerate components DS = detached system PN = central star of a planetary nebula --- u_Type1 Uncertainty flag for object type. --- Type2 Object type number=3 Object type coarsely characterised using the following abbreviations: DD = system consists of two degenerate components DS = detached system PN = central star of a planetary nebula --- Type3 Object type number=3 Object type coarsely characterised using the following abbreviations: DD = system consists of two degenerate components DS = detached system PN = central star of a planetary nebula --- Type4 Object type number=3 Object type coarsely characterised using the following abbreviations: DD = system consists of two degenerate components DS = detached system PN = central star of a planetary nebula --- mag1 Apparent V (B) magnitude at maximum brightness outside eclipse mag f_mag1 B when mag1 is apparent B magnitude --- l_mag2 Limit flag for magnitude mag2 --- mag2 Apparent V (B) magnitude at minimum brightness, in case of eclipses magnitude at mideclipse. mag f_mag2 ":" uncertainty flag on mag2 "B" if mag2 is the apparent B magnitude --- Orb.Per Orbital period d u_Orb.Per Uncertainty flag for Orb.Per --- 2.__Per Spin period of the accretor (white dwarf or neutron star). s EB Flag indicating the occurrence of eclipses number=4 The EB flag means: EB= : (blank) no eclipses observed. EB=1: 1 eclipse per orbital revolution observed. EB=2: 2 eclipses per orbital revolution observed. EB=D: periodic eclipse-like dips observed. --- SB Flag specifying the type of spectroscopic binary number=5 The SB flag means: SB=1: single-line spectroscopic binary SB=2: double-line spectroscopic binary --- SpType2 Spectral type of the secondary number=6 Spectral types are given in the following format: [Spectral class/Luminosity class], where the usual roman numerals for the latter are replaced by the corresponding arabic numerals, i.e. I = 1, II = 2, III = 3, IV = 4, V = 5, VI = 6. --- SpType1 Spectral type of the primary number=6 Spectral types are given in the following format: [Spectral class/Luminosity class], where the usual roman numerals for the latter are replaced by the corresponding arabic numerals, i.e. I = 1, II = 2, III = 3, IV = 4, V = 5, VI = 6. --- l_E Limit flag for the orbital eccentricity --- E Orbital eccentricity --- e_E Error of orbital eccentricity --- M1/M2 Mass ratio M1/M2 --- e_M1/M2 Error of M1/M2 --- l_Incl Limit flag for the orbital inclination --- Incl Orbital inclination deg u_Incl Uncertainty flag for the inclination --- e_Incl Error of orbital inclination deg M1 Primary mass M1 solMass u_M1 Uncertainty flag for primary mass M1 --- e_M1 Error of primary mass M1 solMass l_R1 Limit flag for primary radius R1 --- R1 Primary radius solRad e_R1 Error of primary radius R1 solRad l_M2 Limit flag for secondary mass M2 --- M2 Secondary mass M2 solMass u_M2 Uncertainty flag for secondary mass M2 --- e_M2 Error of secondary mass M2 solMass R2 Secondary radius R2 solRad e_R2 Error of secondary radius solRad References for cbdata.dat (formatted file) References for lmxbdata.dat (formatted file) References for pcbdata.dat (formatted file) References for finding charts (formatted file) Name Object name --- Nref Reference running number for the object number=1 the reference may be absent in file findrefs.dat only, in which case the reference number is blank. --- Text Text of reference (includes the 19-digit bibcode, added at CDS) --- *Variable star names in lexigraphical order Name Object name --- --- --- Names Other names number=1 Catalogue designations involving the equatorial coordinates are given in the following format: HHMMSDDMM (catalogue acronyms) if the position is given in B1950 coordinates JHHMMSDDMM (catalogue acronyms) if the position is given in J2000 coordinates. Here HHMM is the truncated right ascension in hours (HH) and minutes (MM), DDMM the truncated declination in degrees (DD) and arcminutes (MM), and S the sign of the declination. --- *Provisional designations involving constellation names Cname Provisional designation involving constellation name --- --- --- Name Usual name --- *Other names in alphabetical order Desig Common designations --- --- --- Name Main name, or equivalent names --- *Names involving the equatorial coordinates B1950 Name based on B1950 coordinates --- m_B1950 Multiplicity index on B1950 --- J2000 Name based on J2000 coordinates --- m_J2000 Multiplicity index on J2000 --- --- --- Name Main name, or equivalent names --- *References to the catalogue acronyms Abbr Catalogue abbreviation --- Seq Running number within an abbreviation --- Text Text of References (includes the 19-digit bibcode, added at CDS) --- intro.tex Introduction by H. Ritter and U. Kolb (LaTeX, A&A documentclass) cbrefs.txt References for cbdata.dat (text format) lmxbrefs.txt References for lmxbdata.dat (text format) pcbrefs.txt References for pcbdata.dat (text format) findrefs.txt References for finding charts (text format) whoswho.txt *Alternative names of Cataclysmic Binaries contains the 5 parts whoswho1.dat to whoswho5.dat printro.ps *postscript part I (introduction) catpe.ps *postscript part II (description, references) catl.ps *postscript part III (tables; landscape format) H. Ritter, U. Kolb MPA Garching Patricia Bauer CDS 1997 Dec 16 H. Ritter <hsr@mpa-garching.mpg.de> U. Kolb <ulrich@mpa-garching.mpg.de> V_99.xml Catalogue of nearest stars until 10pc 5101 V/101 Nearest stars until 10pc Catalogue of nearest stars until 10pc V A Zakhozhaj Vestnik Khar'kovskogo Universiteta 190 52 1979 1979VKha..190...52Z V/70 : Nearby Stars, Preliminary 3rd Version (Gliese+ 1991) J/other/KFNT/12.20 : Nearby stars metallicities (Zakhozhaj+ 1996) Stars, nearby Stars, masses Stars, diameters Proper motions Parallaxes, spectroscopic Parallaxes, trigonometric Stars, nearby, masses, radii astrometry Spectral types Magnitudes, absolute The given catalogue is a revised version of the catalogue (Zakhozhaj, 1987). The previous numeration is preserved, and the stars, with trigonometric, photometric and spectral parallaxes >0.100" are presented. The catalogue contains data on new components of multiple visual systems, on the components of spectral-binary systems, on invisible components with masses >0.08 solar mass. New data are obtained in 90s and contained in the articles [2-6]. The catalogue contains the main characteristics of stars such as the positions, proper motions, radial velocities, parallaxes, photometrical data and also new data of masses and radii of stars. The completeness of the catalogue is about 70%.
Catalogue of stars within ten parsecs of the Sun Zkh Running number (Zakhozhaj's catalog) --- Name Star identifier --- m_Name Component of multiple star --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin Rem Remark number=1 Coordinates of multiple system components are calculated on the basis of the angular separation and position of observation epoch. --- pmRA Proper motion pmRA.cos(DE) s/yr n_pmRA Notes number=2 *: pmRA and pmDE for multiple system components are calculated by the common proper motion and the position angle. --- pmDE Proper motion pmDE arcsec/a n_pmDE Notes number=2 *: pmRA and pmDE for multiple system components are calculated by the common proper motion and the position angle. --- RV Heliocentric Radial velocity km/s Gliese Gliese (Cat. <V/70>) identifier --- m_Gliese Gliese star component --- Plx Stellar parallax mas n_Plx Index to parallax number=3 t: trigonometric parallax p: photometric parallax s: spectral parallax r: average value of t, p and s parallaxes a: average value of p and s parallaxes o: photometric or spectral parallax --- u_Plx Notes to Plx number=4 *: The values of parallaxes with error of 10% and more. --- l_Vmag Limit flag on Vmag --- Vmag V magnitude mag n_Vmag Note on magnitude number=5 v: variable star S: summarized magnitude of components, n: author' estimation of Vmag and Mv are made for visible component or for component for which it is possible to estimate component spectrum. --- l_Mv Limit flag on Mv --- Mv Absolute magnitude mag n_Mv Note on magnitude number=5 v: variable star S: summarized magnitude of components, n: author' estimation of Vmag and Mv are made for visible component or for component for which it is possible to estimate component spectrum. --- Sp Spectral classification --- n_Sp Notes on spectral class number=6 e: emission lines p: peculiar spectra w: weak spectra lines c: evaluation of spectral class on the basis of known index of colour m: spectra of multiple system component l: luminosity class is estimated by the diagram "colour-luminosity" --- l_Mass Limit flag on Mass --- Mass Mass solMass n_Mass Notes to Mass number=7 t: estimated by the relation of 'mass-effective temperature' c: calculated by the analysis of the line-of-sight curve of spectral binary stars S: summarized mass of seen and unseen components d: calculated by direct methods of mass measurement. w: calculated for white dwarfs by mass-radii relation --- l_Rad Limit flag on Radius --- Rad Radius solRad n_Rad Notes to Rad number=8 t: estimated by the radii-effective temperature relation w: calculated for white dwarfs by mass-radii relation r: calculated by (V-R)-radii relation d: calculated by direct methods of radii measurement ---------------------------------------------------------------------------- References: 1. Zakhozhaj V.A. =1979VKha...190...14...52Z 2. Zakhozhaj V.A. =1982VKha...232...17...64Z 3. Zakhozhaj V.A. 1987, Ph.D.Thesis, Leningrad. 4. Zakhozhaj V.A. =1994KFNT...10b..68Z 5. Zakhozhaj V.A. et al. =1994KFNT...10b..74Z 6. Zakhozhaj V.A. 1995, Astron. Astrophys. Transact. (Moscow), 7, 167 7. Zakhozhaj V.A., Shaparenko E.F. =1996KFNT...12b..20Z --- Veta Avedisova INASAN 1998 Aug 23 V_101.xml SKY2000 - Master Star Catalog - Star Catalog Database, Version 2 5102 V/102 SKY2000 - Master Star Catalog, Version 2 SKY2000 - Master Star Catalog - Star Catalog Database, Version 2 C B Sande W H Warren Jr. D A Tracewell A T Home A C Miller Goddard Space Flight Center, Flight Dynamics Division ??? ??? 1998 1998 SKY2000 - Master Star Catalog - Star Catalog Database, Version 2 J R Myers C B Sande A C Miller W H Warren Jr. D A Tracewell A T Home D A Tracewell Bull. American Astron. Soc., 191, #128.12 ??? ??? 1997 1997AAS...19112812W I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) I/246 : The ACT Reference Catalog (Urban+ 1997) I/250 : The Tycho Reference Catalogue (Hog+ 1998) http://fdd.gsfc.nasa.gov/attitude/skymap.html : Flight Dynamics' Star Catalog Database Positional data Cross identifications Combined data Surveys The SKYMAP Star Catalog System consists of a Master Catalog stellar database and a collection of utility software designed to create and maintain the database and to generate derivative mission star catalogs (run catalogs). It contains an extensive compilation of information on almost 300000 stars brighter than 8.0 mag.
The original SKYMAP Master Catalog was generated in the early 1970's. Incremental updates and corrections were made over the following years but the first complete revision of the source data occurred with Version 4.0. This revision also produced a unique, consolidated source of astrometric information which can be used by the astronomical community. The derived quantities were removed and wideband and photometric data in the R (red) and I (infrared) systems were added. This version, SKYMAP SKY2000 Master Catalog, Version 2 of the SKY2000 Master Catalog was completed in September of 1998 and represents a substantial improvement over Version 1 (see catalog <5095>). A high proportion of the astrometric data in Version 2 comes from ESA's Hipparcos mission, by way of the Hipparcos Output, Hipparcos Component, and Tycho Catalogues. Astrometric data are also present from USNO's ACT Catalog and the European Tycho Reference Catalogue, both of which refine the proper motions in the original Tycho catalog by an order of magnitude. While some objects still retain ACRS and PPM data, the proportion is very small and there are no stars left in the catalog which do not have astrometric quality positions. A large number of photoelectric data on the Johnson system (V, B) has been added from the Tycho Catalogue, such that there are now very few stars in SKY2000 that lack photoelectric data. More than 4000 stars observed by the Ball CT-601 star trackers on the RXTE spacecraft now have observed CCD ST magnitudes in Version 2. IAU designations based on J2000.0 positions have been added to the catalog, while all previous identifiers (SKY2000, HD, SAO, DM, HR, WDS, PPM, AG, bright- and variable-star designations) have been retained. The IAU-approved identifiers allow new objects to be inserted without disrupting the natural order of the principal catalog identifier. There are some deficiencies that exist in the SKY2000 Master Catalog that we are aware of. These items will be researched and corrected in future SKY2000 Master Catalog releases. (See file "deficent.txt").
Data for stars in RA < 1 hour Data for stars in 01 h <= RA < 02 h Data for stars in 02 h <= RA < 03 h Data for stars in 03 h <= RA < 04 h Data for stars in 04 h <= RA < 05 h Data for stars in 05 h <= RA < 06 h Data for stars in 06 h <= RA < 07 h Data for stars in 07 h <= RA < 08 h Data for stars in 08 h <= RA < 09 h Data for stars in 09 h <= RA < 10 h Data for stars in 10 h <= RA < 11 h Data for stars in 11 h <= RA < 12 h Data for stars in 12 h <= RA < 13 h Data for stars in 13 h <= RA < 14 h Data for stars in 14 h <= RA < 15 h Data for stars in 15 h <= RA < 16 h Data for stars in 16 h <= RA < 17 h Data for stars in 17 h <= RA < 18 h Data for stars in 18 h <= RA < 19 h Data for stars in 19 h <= RA < 20 h Data for stars in 20 h <= RA < 21 h Data for stars in 21 h <= RA < 22 h Data for stars in 22 h <= RA < 23 h Data for stars with RA >= 23 h SKY2000 IAU identifier based on J2000 position Field added to SKY2000 Version 1 for SKY2000 Version 2. --- ID Skymap number --- HD Henry Draper <III/135> number --- m_HD HD duplicity indication 1. indicates this the brighter component of a system with a companion >= 0.3 mag. 2. indicates this is the fainter component of a system with a companion <= 0.3 mag. fainter e 9 indicates that this is a blend of two HD stars. The HD number is the lower of the two. --- u_HD HD identification uncertain --- SAO SAO <I/131> number --- m_SAO SAO component --- DM Durchmusterung (BD <I/122>; SD <I/119>; CD <I/114>; CP <I/108>) --- m_DM Durchmusterung supplement letter --- u_DM DM identification uncertain --- HR Harvard Revised <V/50> num. (=BS) --- WDS Washington Double Stars <I/237> number --- m_WDS WDS components --- u_WDS WDS identification uncertain --- PPM Position and Proper Motion number (<I/146>, <I/193>, <I/208>) --- u_PPM PPM identification uncertain --- ID_merg Skymap num. of last skymap entry merged with this star --- name Star name (or AGK3 number) --- var Variable star name (or doubtful variability) --- RAh Right ascension (J2000) hours h RAm Right ascension (J2000) minutes min RAs Right ascension (J2000) seconds s DE- Declination sign --- DEd Declination degrees (J2000) deg DEm Declination minutes (J2000) arcmin DEs Declination seconds (J2000) arcsec e_pos Position uncertainty arcsec n_pos Blended position flag --- r_pos Source of position --- pmRA Proper motion in RA (J2000)/cos(Dec) arcsec/a pmDE Proper motion in Dec (J2000) arcsec/a r_pm Source of proper motion data --- RV Radial velocity km/s r_RV Source of radial velocity data --- Plx Trigonometric parallax arcsec e_Plx Trigonometric parallax uncertainty arcsec r_Plx Source of trigonometric parallax data --- GCI_X GCI unit vector in X (J2000) cos(Dec)*cos(RA) --- GCI_Y GCI unit vector in Y (J2000) cos(Dec)*sin(RA) --- GCI_Z GCI unit vector in Z (J2000) sin(Dec) --- GLON Galactic longitude (B1950) deg GLAT Galactic latitude (B1950) deg Vmag Observed visual magnitude (V or v) mag Vder Derived visual magnitude mag e_Vmag Derived v or observed visual magnitude uncertainty mag f_Vmag Blended visual magnitude flag --- r_Vmag Source of visual magnitude --- n_Vmag V magnitude derivation flag --- Bmag B-magnitude (observed) mag B-V B-V color (observed) mag e_Bmag B or (B-V) magnitude uncertainty mag f_Bmag Blended b-magnitude flag --- r_Bmag Source of b-magnitude --- Umag U-magnitude (observed) mag U-B U-B color (observed) mag e_Umag U or (U-B) magnitude uncertainty mag n_Umag Blended u-magnitude flag --- r_Umag Source of u-magnitude --- Ptv Photovisual magnitude (observed) mag r_Ptv Source of ptv magnitudes --- Ptg Photographic magnitude (observed) mag r_Ptg Source of ptg magnitudes --- Sp_MK Morgan-Keenan (MK) spectral type --- r_Sp_MK Source of MK spectral type data --- Sp One-dimensional spectral class i.e. HD, AGK3, or SAO --- r_Sp Source of one-dimen. spectral class --- sep Separation of brightest and second brightest components arcsec del_mag Magnitude difference of the brightest and second brightest components mag per_orb Orbital period Data for these fields have not been added to the SKY2000 Master Star Catalog. yr PA Position angle deg date Year of observation (AD) yr r_dup Source of multiplicity data --- n_del_mag Passband of multiple star mag. dif. --- dis_near Distance to nearest neighboring star in the master catalog deg dis_2 Dist. to nearest neighboring master cat. star no more than 2 mag. fainter deg ID_A Skymap number of primary component --- ID_B Skymap number of second component --- ID_C Skymap number of third component --- mag_max Maximum variable magnitude mag mag_min Minimum variable magnitude mag var_amp Variability amplitude mag n_var_amp Passband of variability amplitude --- var_per Period of variability d var_Epoch Epoch of var. in JD - 2400000 d var_typ Type of variable star --- r_var Source of variability data --- mag_1 Passband #1-magnitude (observed) mag v-mag_1 v - passband #1 color mag e_mag_1 Passband #1 uncertainty in mag. or col. mag n_mag_1 Passband #1 photometric system Photometry is on the RI system. This byte indicates whether it is Johnson or Russian) --- p_mag_1 Passband #1 Filter used (currently, only R) --- r_mag_1 Source of passband #1: mag. or color --- mag_2 Passband #2-magnitude (observed) mag v-mag_2 v - passband #2 color mag e_mag_2 Passband #2 uncertainty in mag. or col. mag n_mag_2 Passband #2 photometric system Photometry is on the Johnson, Eggen, or Cousins system. This byte indicates which. --- p_mag_2 Passband #2 Filter used (currently, only I) --- r_mag_2 Source of passband #2: mag. or color --- mag1-mag2 Passband #1 - passband #2 color mag f_mag_1 Blended passband #1 mag/color flag --- f_mag_2 Blended passband #2 mag/color flag --- mag_3 Passband #3-magnitude (observed) Fields added to SKY2000 Version 1 for SKY2000 Version 2. The column p_mag_3 contains X, which refers to the star trackers aboard the RXTE satellite. The response curve of these trackers covers the 0.4 to 1.1um range, with its peak sensitivity covering the R and I bands (.65 to .9um) mag v-mag_3 v - passband #3 color mag e_mag_3 Passband #3 uncertainty in mag. or col. mag n_mag_3 Passband #3 photometric system --- p_mag_3 Passband #3 --- r_mag_3 Source of passband #3: mag. or color --- f_mag_3 Blended passband #3 mag/color flag --- *Reference table RefNo Reference number --- n_RefNo Note on the addition of the reference (98) = via SKYMAP Master Star Catalog, Version 3.7 (Cat. <V/77>) .0 = new sources for Version 4.0 .0a = new sources for Version 4.0a +2 = new sources for SKY2000 Version 2 All other sources added for Versions 4.1 and 4.2 --- Text Text of reference The first line contains generally the title, followed by an asterisk (*) when item referenced in the paper, and the number(s) assigned to the catalog in the CDS / ADC Archives within < > The following lines provide the full reference. --- sky.txt Detailed discussion confer.txt Paper prepared for AIAA meeting deficent.txt Known deficiencies Gail L. Schneider ADC/SSDOO 1999 Feb 12 UNKNOWN UNKNOWN Supersedes - SKY2000 - Master Star Catalog CAT #<5095> V_102.xml Line Spectra of the Elements 6016 VI/16 Line Spectra of the Elements Line Spectra of the Elements J Reader Ch H Corliss CRC Handbook of Chemistry and Physics; NSRDS-NBS 68 ??? ??? 1980-1 1981 VI/86 : Bibliography of Atomic Line Identification Lists (Adelman 1996) Spectroscopy Atomic physics This catalog contains wavelength information for 99 different atomic species. The wavelengths for about 46,610 spectral lines of neutral through quadruply ionized atoms are tabulated. The information is presented in a general table of headers and references for each element and for each element a table of relative intensities, wavelengths ordered numerically, chemical elements, and stages of ionization indicated for each line in the wavelength range 40 to 40,000 Angstroms. Listed in the 99 data files are lines that appear in emission from the vacuum ultraviolet to the far infrared. For most atoms these lines are chosen from much larger lists so as to include the stronger observed lines in each spectral region. Below 2000 Angstroms the wavelengths are in vacuum; above 2000 Angstroms the wavelengths are in air. Wavelengths given to three decimal places are suitable for spectrograph calibration purpose such as Ne, Ar, Kr, Fe in the air region and C, N, O, Si, and Cu in the vacuum region. The intensity estimates are useful only as a rough indication of the appearance of a spectrum. The literature references as they appear the the the Handbook of Chemistry and Physics are given in a separate file.
the catalog data Z atomic number --- ion ion --- Int spectral line intensity on arbitrary scale The spectral line intensities for each element are given as a guide to the relative strengths of a line in the spectrum of that element. From element to element and author to author different measures may have been employed to derive these numbers. --- line notes on spectral line --- wavel wavelength in Angstroms 0.1nm Air_Vac flag for wavelength in Air or Vacuum --- Element symbol for element --- Spectrum spectrum of element --- oxide spectral line belongs to oxide ??? --- bwavel truncated wavelength --- note no explanation for this field was given --- refZ reference section --- ref reference number in section --- references to the catalog (refz, ref) refZ Reference section by atomic number --- ref reference number in section --- text reference text In some cases the reference number is missing and the references are ordered by the element and spectrum which then start the reference text separating the identification and reference by a colon. --- Refs. of CRC Handbook of Chemistry and Physics text references to Handbook of Chem. and Phys. --- notes & references to CRC Handbook Ch. & Ph. from original table headers element abbreviated element (alphabetical by element) --- text references to the table of references in file hcp_refs.dat extracted from the original file headers --- Paul Kuin NASA/ADC 1996 Oct 07 UNKNOWN UNKNOWN The original data files contained embedded headers and references. That information for easch elemental data file was extracted and used to create the file refs.dat. In the file notes.dat other information from the table header of each element including the references to the table in the Handbook of Chemistry and Physics are given. These references can be found in the hcp_refs.dat file described above. The brief description for the data was prepared by J. Lyu based on documentation accompanying the catalog. Additional reformatting was done by Paul Kuin (ADC). The original data and text were separated. The data were reformatted and ion number was included. All elements were combined in one data file. The header information was separated to the file refs.dat and notes.dat. Additional notes were included as required in the ReadMe documentation. VI_16.xml UBV Photoelectric Sequences in SA 92-115 6019 VI/19 UBV Photoelectric Sequences in SA 92-115 UBV Photoelectric Sequences in SA 92-115 A U Landolt AJ 78 959 1973 1973AJ.....78..959L Photometry, UBV Photometry, sequences Selected areas The UBV system was originally defined by ten bright standard stars, primarily in the northern sky. These stars are too bright to be used with large telescopes and cannot be reached from southern observatories. This catalog is a careful compilation of data on fainter stars in the equatorial Selected Areas. They are intended as a new set of standards which can be used to define the UBV system at fainter magnitudes in both hemispheres. The stars range in V between 6.0 and 14.9 with most between 9.0 and 13.0.
A discussion of modern broad-band photometric systems has been given by Johnson and Morgan (1953). The stars upon which this system is based are tabulated in Johnson and Morgan (1953), Johnson and Harris (1954) and Johnson (1955,1963). The stars which define the system are nearly all bright stars. The recent large body of southern hemisphere standards (Moreno, Moreno, Stock, Torres and Wroblewski 1966) also consists of bright stars. The stars now recommended for use as UBV standard stars were redefined at the XIVth General Assembly of the IAU to be those objects brighter than V = 5.0 mag between DE = +- 10 deg; however, most of them are still brighter than desirable for the observing techniques and photometers used by most astronomers. There exist, scattered around the sky, photoelectric sequences of fainter stars which are tied into the UBV system. Such sequences, more often than not, are located in galactic or globular star clusters. However, they really are not all on the same precise photometric system, as an intercomparison of two or more observers' data on a given cluster many times shows (see, for example, Landolt 1964); slight zero-point differences and color equation problems occur. Many times, sequences are defined only by one, two or three observations per star. Hence, one ought not use these sequences for extension to fainter objets in extended programs around the sky. There has been much discussion, both privately and in the literature (Blaauw 1955; Walker 1959; Stoy 1958, 1961; Greaves 1955), of the desirability of a faint sequence of standard stars distributed over the sky. Although a variety of useful photometric systems has been established in recent years, the broad-band UBV system still has an important future role in astronomical research. Particularly is this true for the fainter objects to be observed with the big reflectors, where a well defined, widely adopted standard photometric system can be used to great advantage in the initial reconnaissance of faint celestial objects. An attempt is made in this paper to provide a homogeneous set of UBV standard stars in the celestial equatorial Selected Areas. By doing so, astronomers in both hemispheres will have access to faint standard stars readily accessible to the largest telescopes. It is not claimed that this system is a priori better than other fine photoelectric sequences scattered in various regions about the celestial sphere. However, the stars observed herein were thoroughly tied together completely around the sky during many observing sessions from the same site, and using the same type of equipment throughout the duration of the observing program. Therefore, the system should be internally quite accurate and consistent. Many, but not all, of the stars in this catalog are included in later catalogs: 2118 and 2183.
Photoelectric Photometry of Giclas, Feige Stars ID Star Identifications --- RAh Right Ascension (1975) hours h RAm Right Ascension (1975) minutes min RAs Right Ascension (1975) seconds s DE- Declination (1975) sign --- DEd Declination (1975) degrees deg DEm Declination (1975) arcminutes arcmin DEs Declination (1975) arcseconds arcsec V V Magnitude mag B-V (B-V) Color Index mag U-B (U-B) Color Index mag N Number of times star was observed --- M Number of nights star was observed --- e_V V mean error mag e_B-V (B-V) mean error mag e_U-B (U-B) mean error mag rem Note number --- Giclas and Fiege Notes rem Note number followed by period If rem is blank, then note is the continuation from the previous record. --- note Note --- Selected Area Stars area Selected Area Field --- hyphen Hyphen --- ID Star I.D. from Harvard Annals, Vol 101 Durchmusterung of Selected Areas --- RAh Right Ascension (1975) hours (precessed from l900) h RAm Right Ascension (1975) minutes min RAs Right Ascension (1975) seconds s DE- Declination (1975) sign --- DEd Declination (1975) degrees (precessed from l900) deg DEm Declination (1975) arcminutes arcmin DEs Declination (1975) arcseconds arcsec V V magnitude mag B-V (B-V) index mag u_B-V Uncertainty flag on B-V : = uncertain --- U-B (U-B) index mag u_U-B Uncertainty flag on U-B : = uncertain --- N Number of times star was observed --- M Number of nights star was observed --- e_V V mean error mag e_B-V (B-V) mean error mag u_e_B-V Uncertainty flag on e_B-V : = uncertain --- e_U-B (U-B) mean error mag u_e_U-B Uncertainty flag on e_U-B : = uncertain --- BSD Bergedorfer Spektral Durchmusterung ID --- Sp BSD spectral type --- rem Note number --- Selected Area Notes rem Note number followed by a period If rem is blank, then note is the continuation from the previous record. --- note Note --- Spectral Types area Selected Area Field --- hyphen Hyphen --- ID Star I.D. from Harvard Annals, Vol 101 Durchmusterung of Selected Areas -------------------------------------------------------------------------------- Byte-by-byte Description of file: spnotes.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- area Selected Area Field 4 A1 --- hyphen [-]Hyphen 5- 8 I4 --- ID *Star I.D. 10- 80 A71 --- note Note from Harvard Annals, Vol 101 Durchmusterung of Selected Areas --- rem Indicates special note on this star --- Sp MK Spectral type --- Julie Anne Watko SSDOO/ADC 1996 Mar 10 VI_19.xml A finding list for the multiplet tables of NSRDS-NBS 3, Section 1-10 6029A VI/29A Finding list for multiplet tables of NSRDS-NBS 3 A finding list for the multiplet tables of NSRDS-NBS 3, Section 1-10 C J Adelman S J Adelman D Fischel W H Warren Jr. Astron. Astrophys. Suppl. Ser. 60 339 1985 1985A&AS...60..339A Atomic physics Multiplet Spectroscopy The primary references for stellar line identifications in the optical and ultraviolet spectral regions have been "A Multiplet Table of Astrophysical Interest" (RMT, Moore 1945) and "An Ultraviolet Multiplet Table" (UMT, Moore 1950, 1952, 1962). Dr. Charlotte Moore Sitterly has, over the last two decades, undertaken a revision of certain multiplet tables based on data derived from analyses of optical spectra. The present finding list has been prepared from the data published in the first ten sections of these revised tables: -------------------------------------------------- Section Year Elements -------------------------------------------------- 1 1965 Si II, Si III, Si IV 2 1967 Si I 3 1970 C I, C II, C III, C IV, C V, C VI 4 1970 N IV, N V, N VI, N VII 5 1975 N I, N II, N III 6 1972 H I, D I, T I 7 1976 O I 8 1979 O VI, O VII, O VIII 9 1980 O V 10 1983 O IV -------------------------------------------------- An earlier finding list containing Sections 1-7 only was published by Adelman, Adelman and Fischel (1977) (Catalogue VI/11). We have revised the format and added information to the earlier list, and have appended Sections 8-10 to produce the present version. We intend to incorporate future sections to produce new comprehensive lists as the sections are published and can be computerized. This document describes the machine version of the finding list as it is currently being distributed from the Astronomical Data Center. It is intended to enable users to read and process the data without problems and guesswork, and to interpret the various codes used in the list without recourse to the original publications. However, for additional details concerning the multiplet tables and analyses of the optical spectra, the source publications and their associated references should be consulted.
The finding list for multiplet tables El Element (D=Deuterium, T=Tritium). --- Ion Ionisation stage (1=neutral) --- Left a left bracket ([) for predicted wavelength number=1 a wavelength is enclosed in brackets (indicating that a theoretical value of either or both energy levels of the transition has been used to derive the predicted wavelength; [Moore 1967] in the multiplet table). --- lambda Wavelength of the transition (in vacuum for lambda<2000A, in air for lambda>2000A) 0.1nm Right []] a right bracket (]) number=1 a wavelength is enclosed in brackets (indicating that a theoretical value of either or both energy levels of the transition has been used to derive the predicted wavelength; [Moore 1967] in the multiplet table). --- n_lambda See Note number=2 'a' Observed members of series shifted to longer waves by 0.309 A to 0.052 A (n - 5 to 8) when autoionization is effective. 'D' Line deleted in a later publication. 'I' Denotes intersystem combinations of astrophysical interest (see Moore 1965, p. VII for further remarks). 'm' Indicates that the line is masked. The spectrum of the masked line then appears in the intensity column with element identified in bytes 21-22 and atomic species number in byte 26. '*' The line is blended throughout and has more than one classification in the same spectrum (as opposed to appearance in intensity field, byte 23; see explanation for bytes 20-33). '?' for uncertain wavelength --- Ref Reference for the original analysis number=3 The references (letters A to K) are too extensive to be listed in this document and the source publications will need to be consulted if they are required. Users are advised to check the quality of each analysis from which the tables are assembled if uncertainties in identifications are encountered. The same letter codes denote different references in different sections, so the correct section must be consulted. The code "P" indicates a predicted wavelength. --- Int Line intensity number=4 various parts of this data field are uniform, e.g., it is possible to read the numerical intensities if the field is read with format (A3,F6.1,A5) since character data are in all cases separate from numerical intensities. Note, however, that a numerical intensity may be zero or blank, atomic species number may occur in a numerical field if an element is specified in bytes 21-22, and parentheses and asterisks are used to indicate intensity scale changes and that the intensity is affected by that of a neighbouring line or an impurity line. Thus, although numerical intensities may be read and tested upon, the overall data field must be considered for correct interpretation. --- E1 Lower excitation potential number=5 All limits and energy levels given in cm-1 have been multiplied by the factor 0.000123981 to obtain the respective values in eV (see Moore 1965). eV E2 Higher excitation potential number=5 All limits and energy levels given in cm-1 have been multiplied by the factor 0.000123981 to obtain the respective values in eV (see Moore 1965). eV J1 Lower J quantum number --- J2 H1gher J quantum number --- u_J2 A query (?) if the J values are uncertain (appears in source multiplet tables). --- UV "UV" if an ultraviolet multiplet number=6 The letters "UV" when a multiplet occurs shortward of 3000 A and blank for multiplets longward of 3000 A (stated in Moore 1965); however, multiplets having lambda < 3000 A occur throughout the sections without the UV prefix. --- Mult Multiplet number number=7 Due to the retention of earlier numbers from the RMT and UMT, a dual numbering system consisting of real and integer numbers is used (see Moore 1965, p. VII for a more detailed explanation); however, the integer numbers are aligned so that the F format can be used to read them as real numbers. Newly inserted numbers appear in decimal form, while integer numbers only are used after the old multiplet numbers are exhausted. --- Fflag denotes a forbidden transition. --- Blend See Note number=8 A code to indicate blends of specific lines, ultimate lines, italicized numerical intensities, as follows: ------------------------------------------------------------------ A Blended with Ar I C Expanded from single line in multiplet table (multiple J values) D Blend of Si III and Si IV E Blend of N III and N IV G Blend of C I and C II H Blend of C II and C III I Blend of C III and C IV J Blend of C IV and C V K Blend of N IV and N V L Blend of O IV and Si III M Blend of O IV and O V N Blend of O III and O V O Blend of O II and O V P Blend of O VI and O VII Q Blend of O VI and Be III R Blend of O III and O IV S Blend of O II and O IV U Ultimate line (raie ultime) W Blend of N III and N VI X Blend with N II Y Blend with O III Z Blend with Al II 1 Intensity given in italics (significance not found defined in publications) 2 1 + C ------------------------------------------------------------------ --- Sec Section number of HSRDS-NBS 3 publication --- Seq Sequential number of the line in the respective multiplet table. The original tables can be reconstructed by sorting the complete list by Sec,Seq --- Francois Ochsenbein CDS 1995 Aug 30 UNKNOWN UNKNOWN * December 1984, at ADC/NSSDC, by Wayne H. Warren Jr.: Sections 1-7 of the finding list (Adelman, Adelman and Fischel 1977) were available on magnetic tape. The multiplet tables of sections 8-10 were transcribed to data sheets at The Citadel by CJA and SJA, and transferred to disk storage at the ADC by WHW. A format was then designed to accommodate the data of all sections and the differing formats of both groups were changed to the new format. The individual sections were then broken out of the groups for checking. Corrections were made and detailed checks of the original publications performed, the format being revised several times to allow for additional information and to effect homogeneity in the data presentation. Groups of lines which had been added in Sections 1-7 without resequencing were moved to their correct locations and all sections were resequenced to be certain that a sequence sort will recover the original tables exactly. The individual sections were then combined and the complete file sorted by wavelength with secondary sorting on sequence number. * 30-Aug-1995: the printed documentation was converted into an electronic file at CDS. Problems which already occured in Catalogue VI/11 (Sections 1-7) have been corrected in records 4228, 5148, 6957, 7467, and 9951. VI_29A.xml Plate Centers of the European Southern Observatory Sky Survey 6030 VI/30 Plate Centers of the ESO Sky Survey Plate Centers of the European Southern Observatory Sky Survey E B Holmberg A Lauberts H -E Schuster R M West Astron. Astrophys. Suppl. Ser. 18 463 1974 1974A&AS...18..463H Surveys Plate data The "ESO/SRC Atlas of the Southern Sky" is a major tool for, among other things, the optical identification of sources in non-optical wavelengths. It is useful to be able to identify the set of SAO stars in each ESO/SRC survey field both for possible source identifications and for astrometry. The dataset describes the ESO/SRC fields, including the coordinates of the centers. This catalog lists the 606 field centers for the ESO (B) Survey (also called the Quick Blue Survey). For each field are listed field ID, B1950 right ascension (hours and minutes) and declination (whole degrees) followed by right ascension and declination in radians.
Catalog Data FldNum ESO/SRC Atlas of the Southern Sky field number. --- RAh Hours of right ascension. Nominal field center, equatorial coordinates (1950.0), in sexagesimal units. h RAm Minutes of right ascension. min DE- Sign of declination (always minus). --- DEd Degrees of declination. deg RArad Right ascension in radians. Nominal field center, equatorial coordinates (1950.0) in radians. rad DErad Declination in radians. rad C.-H. Joseph Lyu Hughes STX/NASA 1995 Aug 16 UNKNOWN UNKNOWN The file of plate centers (file 1 of this dataset) gives the nominal field centers of the ESO/SRC Atlas of the Southern Sky as listed in Holmberg et al. (1974). This file was prepared by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center. The nominal centers were adopted, and one plate scale was adopted for all the fields. This scale is 66.98 arc seconds/mm in the east-west direction and 67.26 arc seconds/mm in the north-south direction. This scale was derived by measuring the distances between SAO stars on selected films and was tested by generating overlays with a Calcomp plotter. The ability to efficiently generate such overlays for source identification was the primary reason for producing this dataset. VI_30.xml Bidelman-Parsons Spectroscopic and Bibliographical Catalog 6032 VI/32 Bidelman-Parsons Spectroscopic/Bibliographic Cat Bidelman-Parsons Spectroscopic and Bibliographical Catalog S B Parsons N S Buta W P Bidelman CDS Bull. No. 18, p. 86 ??? ??? 1980 1980BICDS..18...86P Combined data Spectral types Bibliography The Bidelman-Parsons Spectroscopic and Bibliographical Catalog (BPSB; Parsons, Buta, and Bidelman 1980a, b) contains data compiled from the astronomical literature by W. P. Bidelman. These data include diverse catalogs and lists, especially from pre-1950 journals (minor as well as major), and from pre-1962 observatory publications. From more recent years, the data on any object frequently are limited to one item with a reference; for example, a spectral type. No data published after 1973 are included. Over 200 publications are represented. The BPSB has information on 40,312 objects. The catalog contains most of the same information on MK spectral types as the Catalogue of Stellar Spectra Classified in the Morgan-Keenan System (Jaschek, Conde, and de Sierra 1964) and its updates, but it also includes such items as spectral types without a luminosity class (certainly better than nothing); spectroscopic absolute magnitudes; notes on multiplicity; notes on high proper motion or radial velocity (with the values, if probably variable, or if greater than 60 km/s); unpublished remarks and spectral types from several sources, including Bidelman and Henize; and Bidelman's preliminary identifications of many sources in the Two-Micron Sky Survey (Neugebauer and Leighton 1969). Some of the longer lists included in the catalog are those of OB stars from the Tonantzintla-Tacubaya and Heidelberg-Koenigstuhl surveys (Iriarte and Chavira 1957; Chavira 1958; Klare and Szeidl 1966); that of OB stars with emission from the Case-Hamburg surveys (Hardorp et al. 1959; Stock, Nassau, and Stephenson 1960; Hardorp, Theile, and Voigt 1964; Nassau and Stephenson 1963; Hardorp, Theile, and Voigt 1965; Nassau, Stephenson, and MacConnell 1965; Stephenson and Sanduleak 1971); and stars from the General Catalogue of Variable Stars (Kukarkin et al. 1969); and the Catalogue of Suspected Variable Stars (Kukarkin et al. 1951, 1965). Although the catalog is mainly of stellar data, it includes many galactic nebulae of various kinds.
First data record for each object ID Identification (based on 1900 position) --- SeqNum Sequence number in group The sequence number of the record within its group (that is, the group pertaining to a given object). --- NumRec Number of records in group The total number of records in the group. --- RAh RA (right ascension) equinox 1900 hours Equinox 1900 coordinates. Either (1) precessed and corrected for proper motion; or (2) from the HD, the GCVS, or another catalog with 1900 coordinates. The BPSB was originally in increasing order by 1900 right ascension, and within each 0.1-minute segment, it is in decreasing (north-to-south) order by declination. Positions given to 0.01 minute of right ascension were ordered as if rounded, with 0.05 minute rounded down. However, the correction of improper values (60 for minutes or seconds and 24 for hours) destroyed this strict order. If two objects have the same coordinates--for example, a planetary nebula and its central star--O.01 minute has been added to one of the right ascensions, in order to make the 1900 coordinates unique for each object. Although the BPSB conventions are somewhat like those of the HD and YBS, they do not preserve the HD and YBS ordering. Note also that the effect of these conventions cannot be reproduced by an ascending character sort on the tag. h RAm RA 1900 minutes min u_RAm uncertainty flag for RA --- DE- Dec 1900 sign, plus (+) or minus (-) --- DEd Dec (declination) 1900 degrees deg DEm Dec 1900 minutes arcmin u_DEm uncertainty flag for DEC --- RAh1950 RA 1950 hours Equinox 1950 coordinates were precessed from 1900, if so indicated by the precession flag; otherwise, taken directly from the source list. For most stars north of declination 88.5 degrees, these coordinates are from the AGK3. h RAm1950 RA 1950 minutes min DE-1950 Dec 1950 sign --- DEd1950 Dec 1950 degrees deg DEm1950 Dec 1950 minutes arcmin Preces Precession flag Precession flag. Colon (:) if 1950 coordinates precessed; otherwise, blank. --- Sp HD spectral type HD spectral type, or a similar one from one of the references (see data2.dat) --- Vmag Visual magnitude In the V or mv or mpv system. Two decimal places are given only when it is clearly a photoelectric V value. mag n_Vmag Note on magnitude : approximate value A or B component of double star C combined value for multiple system This symbol is in the other mag type field, if there is nothing in the other magnitude field. Otherwise, it is in the visual magnitude field itself, in which case the field must be read with an A-type Fortran format. --- Omag Other magnitude, a non-visual magnitude mag n_Omag Type of other magnitude A description of the other magnitude, as follows: B blue in UBV system I near-infrared P mpg (photographic) R red in UBVRI system U ultraviolet in UBV system See also under Vmag above. --- VarMag Minimum mag of variable Minimum magnitude of variable. The magnitude at minimum light of a variable star. If there is another magnitude, this one will usually be of the same type; otherwise, it is usually visual. This field may include a code letter (see above), or a colon (:) meaning upper limit; in these cases, the field must be read with an A-type format. mag HDnum HD number Henry Draper or Henry Draper Extension catalog number. --- HDcode HD code If the object has two HD numbers (e.g., a double star), there is a plus (+) in this byte, and the larger of the numbers is used elsewhere in the catalog. This field may also contain an A or B to differentiate components, or a colon (:) for uncertainty in the identification. --- DMzsign DM zone sign Identifier of the object in the Bonner Durchmusterung (BD), the Cordoba Durchmusterung (CD), or the Cape Photographic Durchmusterung (CPD). This field might also contain some stray Astrographic Catalogue (AC) identifiers, which are similar to those in the Durchmusterungen. This field may also be blank. This applies to stars that have an HD number, but do not have a DM number. This identifier has not been supplied for many HR stars. In the zone around -55, CPD and CD numbers are quite similar in value and could be incorrectly designated. zone sign Plus (+) or minus (-). zone Absolute value of Durchmusterung declination zone. cat code C for CD, P for CPD, or blank for BD. See also under DM above. number The number of the star within its zone. id code May be A or B for BD supplemental stars; P = preceding, or S = succeeding for nearby stars, according to the usage of the AGK2/3; N = north, S = south, P = preceding, F = following for nearby stars, according to another common convention. Caveat emptor. --- DMzone DM zone --- DMcat DM cat code --- DMnum DM number --- DMid DM id code --- Oname Other names Non-HD, non-DM names of the object, separated by commas. Only the one or two most significant of these names will be given for most objects, especially for those with HD numbers. For unfamiliar types of names, consult the references for the object; and in this document, "Appendix A. Catalog Abbreviations" and "Appendix B. Conventions for Greek and Lower-Case Letters" --- Second and subsequent data for the object ID Identification (based on 1900 position) --- SeqNum Sequence number in group See note for data1.dat --- NumRec Number of records in group --- text Free-format text This field contains data and references on the object identified in the first record of the group (see data1.dat). The items are separated by slashes (/). An item may be continued from one record to another. The break between records will occur only adjacent to a blank. If the last non-blank data in a given record is something besides a slash, the item probably continues into the next record. (Or else, the given record is the last one for its object.) Although in a so-called free format, these data do follow a pattern. A typical item can be represented as follows: DATA *REFERENCE (OTHER DATA) The asterisk and parentheses are used literally as shown. Not every element is present in every item. For example, in many cases, only a reference is given. Indeed, sometimes a datum is given with no reference; in which case, one of the other references for the same record probably applies. (Such anomalies are usually the result of uncertainties in interpreting Bidelman's card file, which was accumulated over many years with the aid of student assistants.) Another such case is that of the colon (:), normally used in astronomy to mean approximate; Bidelman's assistants sometimes used this mark to separate a datum from its reference. Some spurious colons have probably made it into the BPSB. Sometimes, there can be two references for the same paper, as for example, if the paper appears both in a journal and in an observatory publication. Here, the second references will be given in parentheses (that is, as "other data"). The reference itself is as follows: journal or other publication, for published data; astronomer's name, for unpublished data; volume or number; page; year (sometimes). In this context, N. is the abbreviation for number. Several references in the same journal volume may be condensed into one reference having a series of page numbers separated by pluses or by commas. See "Appendix C. Publication Abbreviations and Astronomers' Names", and "Appendix A. Catalog Abbreviations" for help in deciphering references. See "Appendix D. Abbreviations Used in the Free-Format Data (data2.dat)" for help in interpreting the data. --- Index (useful only on merged data1 and data2) Name Object name Each index record has one name. For the source of the names, see HD number, DM, and other names under "The First Data Record data1.dat for an Object". Because every name given in the data file is included in the index file, there may be several index records for an object. However, any names that might be given in the free-format data are not included. Only the fields just cited were used. Some objects do not have names. The corresponding index records have the string **NONAME** instead. (These objects can presumably be identified by their coordinates.) The index file is sorted on this field in ascending EBCDIC collating sequence. (The **NONAME** records are at the beginning, in order of 1950 right ascension.) --- RAh RA 1950 hours These coordinates are exactly the same as those in bytes 43-57 of the data file. This field was added because interfacing with other catalogs or databases might require 1950 coordinates in many cases. Note, however, that these coordinates are not guaranteed to be unique to each object, as are the 1900 coordinates, in the data file. h RAm RA 1950 minutes min DE- Dec 1950 sign --- DEd Dec 1950 degrees deg DEm Dec 1950 minutes arcmin flag Precession flag --- FdataRec First data record The sequential number of the first record of the group in data1.dat that pertains question. This number applies only to the complete data file sorted in the original order. --- LdataRec Last data record The sequential number of the last record of the group in data1.dat that pertains to the object name in question. See the remarks under FdataRec. --- C.-H. Joseph Lyu, Nancy Roman, Paul Kuin Hughes STX/NASA 1996 Nov 14 UNKNOWN UNKNOWN The catalog was originally maintained on three-by-five-inch index cards. In 1973, NASA Experiment S-019 purchased a photocopy, which resides at the University of Texas in Austin. There, the data were keypunched and written to magnetic tape. In February, 1980, the catalog was received from the University of Texas by the Astronomical Data Center (ADC), NASA/Goddard Space Flight Center. Several major changes in the format of the catalog (none in the contents) were made by one of the present authors (Hill) under ADC auspices. The resulting catalog is described in this document. The two most important features of the original catalog were its condensed format, and its division into multiple files. The data were in a single stream that continued freely over record and block boundaries. The beginning and end of the data for each object were indicated with special character strings, as were the beginning and end of each particular data item. The data were divided into 96 files, each one covering 15 minutes of right ascension. This process was accomplished in three steps, each done by means of a Fortran program: 1. A file of variable-length records was generated with one object per record, but with the data otherwise in the original stream format. 2. The format was converted to the present one, with several fixed-length records per object. The tag at the beginning of each record was generated. 3. The index file was generated. Appendix A. Catalog Abbreviations: Abbreviations in capital letters for the names of publications are listed in "Appendix C. Publication Abbreviations and Astronomers' Names" Abbrev. IAU Abbreviation and Notes AC Astrographic Catalogue (Carte du Ciel) Publ. by 18 observatories in 141 volumes, 1902-1963. ADS R. G. Aitken, New General Catalogue of Double Stars within 120 Degrees of the North Pole. Carnegie Institution of Washington, 1932. AG Catalog der Astronomischen Gesellschaft. 19 volumes, Leipzig, 1890-1912. AGK2 R. Schorr and A. Kohlshuetter, Zweiter Katalog der Astronomischen Gesellschaft. 15 volumes; Hamburg-Bergedorf Sternwarte, 1951-1958. AS(MWC) P. W. Merrill and C. G. Burrwell, 1950, APJ 112, 72. W. C. Merrill and P. W. Merrill, 1951, APJ 113, 624. BD Bonner Durchmusterung. 4 volumes; first edition, 1859-1862; second edition, 1903, includes "a" a~d "b" stars. BGC S. W. Burnham, A General Catalogue of Double Stars within 121 Degrees of the North Pole. Carnegie Institution of Washington, 1906 BOSS L. Boss, Preliminary General Catalogue of 6188 Stars for the Epoch 1900. Carnegie Institution of Washington, 1910. BPM W. J. Luyten, Bruce Proper Motion Survey: the General Catalogue. 2 volumes; Minneapolis, University of Minnesota, 1963. BSD A. Schwassman and P. J. van Rhijn, Bergedorfer Spektral- Durchmusterung. 5 volumes; Hamburg. Sternw., 1935-1953. (same as BERGD in "Appendix C. Publication Abbreviations and Astronomers' Names") V Bamberg variable (see esp. IBVS references) C (see COD) CASE J. J. Nassau and V. M. Blanco, 1954, APJ 120, 129; 1957, APJ 125, 195. V. M. Blanco, 1958, APJ 127, 191. CI(18) J. G. Porter, E. I. Yowell, and E. S. Smith, 1918, Publ. Cincinnati Obs. No. 18, pt. 4. CI(20) --------, 1930, Publ. Cincinnati Obs. No. 20. COD Cordoba Durchmusterung. 5 volumes; Res. Obs. Nac. Argent. 16-18, 1892-1900; 21, pts. 4 & 5, 1914-1932. CPD Cape Photographic Durchmusterung. CAPE OBS ANN 3-5, 1896- 1900. DM (see BD, COD, or CPD) F J. Feige, 1958, APJ 128, 267. G H. L. Giclas, R. Burnham Jr., N. G. Thomas, LOWELL B No. 89 - No. 162, 1958-1975. ( 18 lists) GC B. Boss, General Catalogue of 33342 Stars for the Epoch 1950. Carnegie Institution of Washington, 1937. GD H. L. Giclas, R. Burnham, Jr. and N. G. Thomas, LOWELL B No. 125, No. 141, No. 153, No. 158, No. 160, No. 162.; 1965-1975. GL W. Gliese, HEID MITT No. 22, 1969. (Catalogue of Nearby Stars) GMB S. Groombridge, Catalogue of Circumpolar Stars for 1810. London, 1838. GR H. L. Giclas, R. Burnham, Jr., and N. G. Thomas, LOWELL B No. 158, No. 160, No. 162; 1972-1975. GR (see GMB) GR AST (see AC, Greenwich volumes) HD Henry Draper Catalogue. HA 91-100, 1918-1936; HA 112, 1949. HR D. Hoffleit, Catalogue of Bright Stars. Yale University Obs. 1962 (3rd revised edition). ( BS = HR) I (see IC) IC Index Catalogue of Nebulae and Clusters; Second Index Catalogue of Nebulae and Clusters. (see NGC) K (see KZP) KZP B. V. Kukarkin, et al., Catalogue of Suspected Variable Stars. Moscow, Academy of Sciences of the USSR; first catalogue, 1951; second catalogue, 1965. (in Russian) KW W. J. Klein-Wassink, 1927, GRaN PUB No. 41. LB W. J. Luyten et al., A Search for Faint Blue Stars, No. 1-42. Minneapolis, Lund Press, 1955-1966. LDS W. J. Luyten, 1941, Publ. Obs. U. Minn., III, No. 3. LEE 0. J. Lee et al. 1943, DEARBORN 4, pt. 16; 1947, DEARBORN 5, pts. 3 and 7. LFT W. J. Luyten, A Catalogue of 1849 Stars with Proper Motions Exceeding 0.5 Arc Seconds Annually. Minneapolis, Lund Press, 1955. LK H ALF G. H. Herbig, 1954, APJ 119, 483; 1954, PASP 66, 19; 1956, PASP 68,353; 1957, APJ 125, 654; 1958, APJ 128, 259; 1960, APJ SUPP 4, 337; 1960, APJ 131, 516; 1961, APJ 133, 337; 1962, Adv. Astr. Astrophys. 1. 47. G. H. Herbig and L. V. Kuhi, 1962, APJ 137, 398. M. L. Walker, 1961, APJ 133, 438. LP W. J. Luyten et al., Proper Motion Survey with the Forty-eight Inch Schmidt Telescope, No. 1 - No. 42. Minneapolis, University of Minnesota, 1963-1975. LS Luminous Stars in the Northern Milky Way, I-VI. Hamburg- Bergedorf, 1959-1964. (LS is followed by the volume number) LTT W. J. Luyten, A Catalogue of 9867 Stars in the Southern Hemisphere with Proper Mothins exceeding 0.2 Arc Seconds Annually. Minneapolis, Lund Press, 1957. -------, A Catalogue of 7127 Stars in the Northern Hemisphere with Proper Mothins exceeding 0.2 Arc Seconds Annually. Minneapolis, Lund Press, 1961. MCC A. N. Vyssotsky et al. 1943, APJ 97, 381; 1946, APJ 104, 234; 1952, APJ 116, 117; 1956, AJ 61, 201; 1958, AJ 63, 211. MWC P. W. Merrill and C. G. Burrell 1933, APJ 78, 87; 1943, APJ 98, 153; 1949, APJ 110, 387. (Erratum, 1949, APJ 111, 666). MSB P. W. Merrill, R. F. Sanford and C. G. Burwell 1933, PASP 45, 306. M C. Messier, 1787. (see any introductory astronomy textbook) N (number of star in one of the references, or within a star cluster) NGC J. L. E. Dreyer, New General Catalogue of Nebulae and Clusters, 1888; Index Catalogue of Nebulae and Clusters, 1895; Second Index Catalogue of Nebulae and Clusters, 1905; reprinted in MEM RAS, 1953. (first catalogue only is NGC; other two are IC) NPS A. J. Cannon 1917, HA 71, No. 3. P (see CPD) R R. A. Rossiter 1955, MICH PUB 11, 1. ROSS F. E. Ross, AJ 36, 96 - AJ 48, 163; 1925-1939. (12 lists) S Sonneberg variable (see esp. MVS references) SA Selected Areas (see BSD) VY (see MCC) VYS (see MCC) VAN B G. van Biesbroeck 1961, AJ 66, 528. W G. Westerhout 1958, BAN 14, 215. WOLF M. Wolf 1919, Veroff. Sternw. Heidelberg 7, 195 (No. 10); AN No. 4996 - No. 5658, 1919-1929; (31 lists). WRA J. D. Wray 1966, Dissertation, Northwestern University (Table 15). (see partial list in L. R. Wackerling 1970, Mem RAS 73, 153). Variables i. e., variable-star names like R AND, RR AND, or V335 AND B. V. Kukarkin et al., General Catalogue of Variable Stars. Moscow, Academy of Sciences of the USSR; first edition, 1948; second edition, 1958 (2 volumes and supplement, 1960); third edition, 1969 (3 volumes and 3 supplements, 1971, 1974, 1976). (form of designation: a three-letter constellation abbreviation preceded by a single letter R-Z; or double letters RR-RZ, SS-SZ, ... ZZ, AA-AZ, ... BB-BZ, ... QQ-QZ (J not used); or the letter V plus a number greater than or equal to 335.) (see also IBVS references) Appendix B. conventions FOR GREEK AND LOWER-CASE LETTERS: -------------------- Greek Representation -------------------- alpha ALF beta BET gamma GAM delta DEL epsilon EPS zeta ZET eta ETA theta THT iota IOT kappa KAP lambda LAM mu MU nu NU xi XI omicron OMI pi PI rho RHO sigma SIG tau TAU upsilon UPS phi PHI chi CHI psi PS omega OMG -------------------- The Centre de Donnees Stellaires (CDS) in Strasbourg, France, has adopted TET instead of THT, and KHI instead of CHI. A lower-case letter is indicated with a period; for example, e Car is represented as L. CAR. This type of name is generally omitted from the BPSB, if not used in the Catalogue of Bright Stars, or in the GCVS. (See HR, and Variables in "Appendix A. Catalog Abbreviations") APPENDIX C. PUBLICATION ABBREVIATIONS AND ASTRONOMERS' NAMES: An abbreviation in the right-hand column beginning with a single left parenthesis [(] refers to a publication not in the International Astronomical Union list (Pecker 1966). ------------------------------------------------------------------------------ Abbr. IAU Abbreviation ------------------------------------------------------------------------------ A ZH Astr. Zu. AAP (Astr. Astro-phys. [1892-1894] ABAST BULL Abastumansk. Ap. Obs. Gora Xanobili Bjull. ACT AST SINICA Acta Astr. Sin. ACTA ASTR Acts Astr. ADV A+A Adv. Astr. Astrophys. AJ Astr. J. ALLEGH PUB (Publ. Allegheny Obs., Univ. Pittsburgh [AO] ALMA-ATA Izv. Akad. Nauk Kazah. SSR Ser. Fiz. Mat. Nauk Astrofiz. AMST PROC K. Ned. Akad. Wet. Proc. Sect. Sci. Ser. B AMSTERDAM Publ. Astr. Inst. Univ. Amsterdam AN Astr. Nachr. ANKARA Commun. Dep. Astr. Ankara Univ. ANN AP Ann. Astrophys. ANN FENN (Ann. Acad. Sci. Fennicae ANN REV A. Rev. Astr. Astrophys. ANN SOLAR PHYS OBS (Ann. Solar Phys. Obs. [Cambridge] AP LETT (Astrophys. Letters AP SP SCI (Astrophys. Space Sci. APJ Astrophys. J. [Lett. Sec.: L---] APJ SUPP Astrophys. J. Suppl. Ser. ARCETRI PUB Osserv. Mem. Oss. Astrofis. Arcetri ARK AST Ark. Astr. [Arkiv... Stockholm] ASIAGO CONT Contr. Oss. Astrofis. Univ. Padova [Asiago] ASOC ARG Asoc. Argent. Astr. Bol. ASTR CIRC Astr. Cirk. Izdav. Bjuro Astr. Soobsc. Kazan ASTRON Astronomie A+A (Astr. Astrophys. [1969- ] A+A SUPP (Astr. Astrophys. Suppl. BA Bull. Astr., Paris BAAS (Bull. Am. Astr. Soc. BABELSBERG Veroff. Sternw. Babelsberg [Berlin] BAC Bull. Astr. Inst. Csl. BAMBERG KL Kleine Veroff. Remeis-Sternw. =KVB [Bamberg] BAMBERG VER Veroff. Remeis-Sternw. Bamberg BAN Bull. Astr. Inst. Netherl. BASIC AST DATA (Basic Astr. Data, 1963, Ed. K. Aa. Strand BERGD (Hamburg. Sternw. - Bergedorfer Spektral-Durchm. BERL MONATS (Monatsberichte Preuss. Akad. Berlin BI --see names below BOSSCHA ANN Ann. Bosscha-Sterrenw. [Lembang] BOSSCHA CONT Contr. Bosscha Obs. [Lembang] BS CAT (Hoffleit, D., Catalogue of Bright Stars BULL PETERSB (Bull. Acad. Imp. Sci. St.-Petersbourg BURAKAN Soobshch. Bjurak. Obs. BZ (Beobachtungs-Zirkular der Astr. Nachr. CAPE --> MN 129, 63 (1964) CAPE MIM (Cape Obs. Mimeogram CAPE OBS ANN Ann. Cape Obs. CAR YB (Carnegie Ybk. = Ann. Rept. of Mt. W. + Pal. Obs. CATANIA PUB Oss. Astrofis. Catania Publ. (N. 3 --> MEM SOC IT 26, 409) CIEL TERRE Ciel et Terre CIR (Caltech Two-Micron Sky Survey, NASA SP-3047 COD CAT (Cordoba Durch. [intro.] COL CONTR (Rutherford Obs. Contr. [No. 32] [Columbia Univ.] COMM ESO Commun. Europ. Sth. Obs. COPENHAGEN Publ. Mind. Medd. Kbh. Obs. CR C. R. Acad. Sci. Paris [Comptes Rendus] CRIM A O Izv. Krym. Astrofiz. Obs. DAO Publ. Dom. Astrophys. Obs., Victoria DAO CONT Contr. Dom. Astrophys. Obs., Victoria DDO COMM Commun. David Dunlap Obs. DDO PUB Publ. David Dunlap Obs. DEARBORN Ann. Dearborn. Obs [V. 4, 5] DENMARK (Mem. Akad. Roy. Sci. and Letters, Denmark DOM OBS CONT Contr. Dom. Obs., Ottawa DOM OBS PUB Publ. Dom. Obs., Ottawa [DO] FRANKFURT VER (Veroff. Astr. Inst. Univ. Frankfurt GCVS (General Catalogue of Variable Stars GENEVE PUB Publ. Obs. Geneve GOTTINGEN (Astr. Mitt. Ronigl. Sternw. Gottingen GOTT MITT Veroff. Univ. Sternw. Gottingen GRON PUB Publ. Kapteyn Astr. Lab. (Groningen) H P PUB Publ. Obs. Hte-Provence HA Ann. Harv. Coll. Obs. HAC Harvard Coll. Obs. Announc. Cards HAMBURG Mitt. Hamburg. Sternw. [Bergedorf--recent] HAMGBURG ABH Astr. Abh. Hamburg. Sternw. Bergedorf HARV REPR Harvard Repr. HB (Bull. Harv. Coll. Obs. HC (Circ. Harv. Coll. Obs. HDC NOTE (Henry Draper Catalogue notes HEID-KONIG (Ver. Landessternw. Heidelberg-Konigstuhl [Vol. 18] HEID MITT Astr. Rechen-Inst. Heidelb. Mitt. A, B HEID PUB Veroff. Astr. Rechen-Inst. Heidelberg IAU SYMP (IAU Symposium IAUC (IAU Announc. Cards IBVS Comm. 27 IAU Inf. Bull. Var. Stars [VSB] INDIANA PUB Publ. Goethe Link Obs. [Indiana] IRISH AJ Irish Astr. J. JBAA J. Br. Astr. Ass. JDO J. Observateurs JRASC J. R. Astr. Soc. Can. KIEL Sonderdr. Sternw. Kiel KNOW (Knowledge KPNO CONT Kitt Peak Nat. Obs. Contr. KVB Kleine Veroff. Remeis-Sternw. [Bamberg] =BAMBERG KL LAWS OBS (Laws Obs. Bull. [Univ. Missouri Bull.] LA PLATA Obs. Astr. Univ. Nac. La Plata Ser. Astr. LA PLATA B Publ. Astr. Univ. Nac. La Plata LA PLATA C (Astr. Univ. Nac. La Plata Circ. LEIDEN Ann. Sterrew. Leiden LICK Publ. Lick Obs. LIEGE PUB Univ. Liege Inst. Astrophys. Coll. 4 (Coll. 8) LIEGE REPR Univ. Liege Inst. Astrophys. Coll. 4 (Coll. 8) LOB Lick Obs. Bull. LOW LUM STARS (Symp. on Low-luminosity Stars, 1968, Univ. Virg., ed. Kumar LOWELL B Lowell Obs. Bull. LS I - VI (Lum. Stars Northern Milky Way LTT (Cat. Proper Motions Exc. 0.2, Luyten [See "Appendix A. Catalog Abbreviations"] LUND MEDD Medd. Lunds Astr. Obs. LYON ANN Ann. Univ. Lyon MADRID AN (Madrid Annario MAGNETIC STARS (Mag. & Related Stars, 1967, Mono Press, Ed. Cameron MCC PUB Publ. Leander McCormick Obs. [Univ. Virginia] MEDD ROEMER OBS Medd. Ole Romer Obs. [Aarhus] MEM CO (Mem. Commonwealth Obs. [Mt. Stromlo] MEM RAS Mem. R. Astr. Soc. MEM SOC IT Mem. Soc. Astr. Ital. MEM SPETTA IT (Mem. Soc. It. Spectrosc. MICH PUB Pub. Obs. Univ. Michigan MICH REPR Obs. Univ. Michigan Repr. MILANO CONT Contr. Oss. Astr. Milano-Merate MILANO PUB Pubbl. Oss. Astr. Milano-Merate MINN PUB Publ. Astr. Obs. Univ. Minnesota MITT PULK (Pulkovo Mitt. MITT UNGAR Mitt. Sternw. Ungar. Akad. Wiss. MKK ATLAS (Atlas of Stellar Spectra, 1943, Morgan, Keenan, Kellman MN Mon. Not. R. Astr. Soc. MNASSA Mon. Notes Astr. Soc. 5th. Afr. MORPH ASTR (Morphological Astronomy, Zwicky MT W COMM (Commun. Mt. Wilson Solar Obs. MT W CONTR (Contr. Mr. Wilson Qbs. MT W REP =CAR YB MVS Mitt. Veranderl. Sterne [Sonneberg] NATURE Nature NEB INT (Nebulae & Interstellar Matter, 1968, ed. Middlhurst & Aller OBS Observatory OBS BEL BULL Bull. Astr. Obs. R. Belgique OBS BELG COMM Commun. Obs. R. Belgique OBS PARIS (Ann. Obs. Paris PA Pop. Astr. PAAS (Publ. Am. Astr. Soc. PADOVA CONT Contr. Oss. Astrofis. Univ. Padova PASJ Publ. Astr. Soc. Japan PASP Publ. Astr. Soc. Pacific PAT (Pop. Astr. Tidschrift PENN PUB Publ. Univ. Pa. Astr. Ser. [Flower & Cook Obs.] PERKINS Contr. Perkins. Obs. [Ohio Wesleyan] PETERSB MEM (Mem. Acad. St. Petersburg PHIL TRANS Phil. Trans. R. Soc. Lond. A PNAS Proc. Nat. Acad. Sci. USA POTSDAM Publ. Astrophys. Obs. Potsdam PRIN CONT (Contr. Princeton Univ. Obs. PRINCETON (Publ. Princeton Univ. Obs. PROC EDINB Proc. R. Soc. Edinburgh PROC RS Proc. R. Soc. London PUB LYON Publ. Obs. Lyon PUB USNO Pubs. U. S. Nav. Obs. PULK OBS C (Pulkovo Obs. Circ. PULKOVO BULL (Bull. Pulkovo Obs. [Translation] PULKOVO PUB Izv. Glav. Astr. Obs. Pulkovo PZ Perem. Zvezdy [VS] R OBS ANN (R. Obs. Ann. [Greenwich] RASC HANDB (Observers Handbook, R. Astr. Soc REND ACC LINC Atti Accad. Naz. Lincei Rc. [Roma] REP OBS C Republ. Obs. Johannesb. Circ. RIC ASTR Ric. Astr. Spscola Astr. Vatic. RO PUB Publ. R. Obs. Edinburgh ROB R. Obs. Bull. [Greenwich] RSA (Rev. Soc. Astr. Espana y America RUSS ASTR GES (Nach. Russ. Astr. Ges. RV CAT (Gen. Cat. Stellar Rad. Vel., Wilson, 1953 SID MS (Sidereal Messenger SKY+TEL Sky Telesc. SONN Veroff. Sternw. Sonneberg [VSS] SOVIET ASTR Soviet Astr. STELL ATM (Stellar Atm., 1960, ed. J. L. Gr STERNB PUB Trudy Gos. Astr. Inst. Sternberga STERNE Sterne [Leipzig] STOCKHOLM Stockholm Obs. Ann. STOCKHOLM MEDD Stockholm Obs. Medd. STROMLO MIM (Mt. Stromlo Mimeogram STROMLO REPR Mt. Stromlo Obs. Repr. TASHKENT BUL (Bjull. Tashkentskoi Astr. Obs. TOKYO BULL Tokyo Astr. Bull. TOKYO REPR Contr. Dep. Astr. Univ. Tokyo TOULOUSE Ann. Obs. Astr. Met. Toulouse TORUN OBS BULL Bull. Astr. Obs. Univ. N. Coper. TRANS EDINB Trans. R. Soc. Edinburgh TRANS IAU Trans. IAU [Pub. IAU] TRUDY INST AP Trudy Inst. Astrofiz. Stalinabad T+T BOL Bol. Obs. Tonantzintla Tacubaya UNION OBS CIRC Union Obs. Circ. UPPS MEDD Uppsala Astr. Obs. Medd. VAN VLECK Publ. Van Vleck Obs. [Wesleyan Univ.] VAR STAR N Z (Var. Star Circ. New Zealand VAT Ric. Astr. Specola Astr. Vatic. / (Vat. Obs. Pub. VFPA (Verein Freunden Physik Astr. Gorki (Verand. Sterne) [Nishni-Novgorod] VILNIUS Astr. Obs. Biul. Vilnius VISTAS (Vistas in Astr., ed. A. Beer VJS (Vierteljahrschrift Astr. Gesell. WASHBURN (Publ. Washburn Obs. Univ. Wisconsin [WO] W+S (Publ. Warner & Swasey Obs. [Lum. Stars. 5th. Milky Way] YALE Trans. Astr. Obs. Yale Univ. YERKES Publ. Yerkes Obs. ZFA Z. Astrophys. ------------------------------------------------------------------------------ Names for unpublished data (sometimes published later): Abt, H. A. Albers, H. Aller, L. H. (Astrophysics, 1954) Barbier, M. BI = Bidelman, W. P. Bond, H. E. Bouigue, R. (Ann. Ap. 17, 104) Buscombe, W. Cowley, A. Cowleys, A., C. (PASP 77, 184) Dean, C. Deeming, T. Duke, D. Duner, N.-C. (Mem. on Stars of Secchi's 4th Type) Dworetsky, M. M. Edmondson, F. K. Espin, T. E. Feast, M. Finsen, W. S. Frye, R. L. Hardorp, J. (A+A 22, 129, 1973) Haro, G. Henize, K. G. Herbig, G. H. Hiltner, W. A. Hoffleit, D. Houk, N. Innes, R. T. A. (southern double stars) Jaschek, C., M. Joy, A. H. Keenan, P. C. Kelsall, T. Kron, G. E. Krueger, F. Kuiper, G. P. Lee, O. J. (see "Appendix A. Catalog Abbreviations") Lynga, G. MacConnell, D. J. Mayall, N. U. Minkowski, R. Murphy, R. Osawa, K. Perry, C. Pesch, P. Roberts, M. Robinson, J. Roman, N. G. Rybski, P. M. Sanford, R. F. (ApJ 99, 145) Santirocco, R. (U. Rochester thesis) Secchi, A. Slettebak, A. Smith, Henry J. (Harvard thesis) Stephenson, C. B. Thackeray, A. D. Wallerstein, G. Warner, B. Wray, J. D. APPENDIX D. ABBREVIATIONS USED IN THE FREE-FORMAT DATA: -------------------------------------------------- Abbrev. Meaning -------------------------------------------------- A] component A of double star ABS absorption APS apsidal ASTR BIN astrometric binary B] component B of double star BIN binary star BR] brighter component of double star BR bright (emission) BRT bright (emission) CE continuum emission CHAR character. characteristic CI color index CL cluster CMP composite spectrum COL color indices COMP composite spectrum, companion, component COMP SE comparison sequence CON continuum, continuous spectrum CONT continuum, continuous spectrum CPM common proper motion C STAR supergiant star, carbon star CT Cerro Tololo Obs. DBL double star DEG degrees (of arc, of temperature) DELTA CEP Cepheid variable star DELTA DEL Delta Del-type spectrum DEL DEI Delta Del-type spectrum DELTA M Delta(m) (difference in magnitude between double-star components) DEL M Delta(m) (difference in magnitude between double-star components) DIAM diameter DIFF diffuse nebula DYN PI dynamical parallax ECL eclipsing (binary), eclipse EM emission EW equivalent width FT faint FT) fainter component of double star GLOB CL globular cluster GT greater than HALO halo-population object H-B horizontal branch HK CaII H and K lines HOR-B horizontal branch HOR BRANCH horizontal branch ID identification IDENT identification INCL included in, member of INT interstellar absorption lines INT intensity IR infrared KPS kilometers per second LE line emission LICK PL Lick Obs. plate no. LT less than M mv (apparent visual magnitude) MET metal lines (spectral type from -- ) MF magnetic field MSCH PL University of Michigan Obs. plate no. MIN minutes of arc ML metal lines (spectral type from --) MOD moderate MPG mpg (apparent photographic magnitude) MSP absolute magnitude (spectroscopic) MU proper motion MV visual absolute magnitude NEB nebulosity OBJ PR objective prism OCC occultation OCCULT occultation OP objective prism OPT optical ORB orbit P period P CYG P Cygni-type spectrum PEC peculiar PHOT photometry PHOTO photograph PHOTOM photometry PI parallax PI (DYN) dynamical parallax PI (SP) spectroscopic parallax PL plate number POL polarization POSS possible, possibly RAD radiation RED reddening, reddened REDD reddening, reddened RHO separation (between two objects) ROT v sin i (projected rotational velocity) R, R-I photometric R and I colors, indices RV radial velocity SB spectroscopic binary SEC seconds of arc, second, secondary SEP separation (between two objects) SL slightly SP spectrum STR strong SYMB symbiotic (combination) spectrum TOLOLO Cerro Tololo Obs. UBV photometric U, B, and V colors [UBV] spectral type was estimated from UBV colors UV ultraviolet V very VAR variable VIS visual W[H GAM] H_gamma equivalent width WK weak -------------------------------------------------- VI_32.xml A Multiplet Table for MnI 6034 VI/34 A Multiplet Table for MnI A Multiplet Table for MnI S J Adelman G F Svatek K Van Winkler W H Warren Jr. Astron. Astrophys. Suppl. Ser. 80 285 1989 1989A&AS...80..285A Multiplet Spectroscopy Atomic physics Finding lists The machine-readable version of A Multiplet Table for MnI contains data on excitation potentials, J values, multiplet terms, intensities of the transitions, and multiplet numbers. Files ordered by multiplet and by wavelength are included.
A Multiplet Table for Mn I was prepared by first calculating all possible transitions consistent with a change in J of 0, -1, and +1 from the atomic energy levels of Mn I (Corliss and Sugar 1977). The transitions selected for inclusion were observed lines from Cataln, Meggers, and Garcia-Riquelme (1964), Brown and Ginter (1978), and Baig, Connerade, and Newson (1979). Also included were predicted lines to complete multiplets in which one or more lines were seen by Cataln et al. (1964) and predicted multiplets contained in Kurucz and Peytremann (1975). These predicted transitions satisfy L-S coupling rules. Users should consult the source publication and the references to the original work that are cited in the bibliography at the end of this document for additional details.
Multiplet Order Wavelength Order Mn Element (Mn) --- spec Atomic species number ( 1) --- lam Wavelength Wavelength of the transition. They are in air except shortward of 0.2 mu, where they are in vacuum. Note that the precision varies (the last two bytes can be blank). 0.1nm ref Reference code The reference codes are as follows: A = Catalaen et al. (1964) B = Based on gf values of Kurucz and Peytremann (1975) using values of Catalaen et al. (1964) as a guide for lines of similar excitation potential C = Brown and Ginter (1978), but divided by 10 D = Baig et al. (1979) P = Predicted line Users are advised to check the quality of each analysis from which the tables were assembled if uncertainties in identifications are encountered. --- int Laboratory intensity This data field is divided into several uniform parts, the wide spacing being required to isolate the various segments of the field. Thus, it is possible to read the numerical intensities by using the format specification (A3,F6.1,A5) because character data are, in all cases, separate from the numerical intensities. Note, however, that a numerical intensity may be zero or blank. Also note that decimal points have been added to integer intensities so that the numerical field is always either a real number of blank. Parentheses in bytes 20 (left) and 32 (right) are used to indicate intensity scale changes and an asterisk (*) in byte 33 denotes that an intensity is affected by that of a neighboring, or impurity, line. Although numerical intensities may be read and tested upon or sorted, the overall data field must be considered for correct interpretation. --- low_ex Lower excitation potential All limits and energy levels given in inverse centimeters have been multiplied by the factor 0.000123981 to obtain the respective values in electron volts (see Moore 1965). eV high_ex Higher excitation potential eV low_J Lower J value Value corresponding to the low level involved in the transition producing the line. --- high_J Higher J value Value for high level. There is no specific secondary order of J values in the wavelength-ordered file when multiplet lines at an identical wavelength occur; i.e., no secondary sorts were attempted beyond that on wavelength, since there is no rational way to order the lines beyond wavelength. --- low_term Lower term designation Term designations from the source material, without the J values attached to them. The complete upper state designations from Brown and Ginter (1978) and Baig et al. (1979) are not given for lack of space, and some multiplets represent lines with unclassified upper states grouped together for convenience. These include many multiplets between UV 2.88 and UV 2.343. --- high_term Higher term designation --- code Code The following codes are employed: A = Indicates a change from Catalaen et al. (1964), e.g., by the inclusion of additional lines of the same wavelength and differing J values, and where the upper limit term has been changed. B = Major component. --- code_UV Code for UV The letters UV when a multiplet occurs shortward of 0.3 microns (stated in Moore 1965). However, multiplets having wavelength < 0.3 microns occur without the prefix and a few multiplets just longward of 0.3 microns contain the prefix. --- mult Multiplet number Older multiplet numbers, as used in RMT and UMT, are used wherever possible. New multiplet numbers begin with 61. Note that the dual numbering system described by Moore (1965) (see p. vii) is used in principle, but that decimal points have been added to the integers so that all numbers are uniform in format. --- for_code Forbidden transition code The letter F indicates a forbidden transition. --- no Sequential number The multiplet-ordered table was assigned a sequential numbering to provide an independent means of ordering the table. This was done because if the multiplet table is disordered, it is virtually impossible (at least we couldn't find a way) to reorder it by machine sorting. The sequential numbers are, of course, retained in the wavelength-ordered table to indicate where the lines are located in the multiplet table. --- Nancy G. Roman ADC/SSDOO 1995 May 15 The partial support of The Citadel Development Foundation toward the computerization of the tabular data is gratefully acknowledged. UNKNOWN UNKNOWN The data were compiled and computerized by S. J. Adelman, G. F. Svatek, and K. Van Winkler with financial support from The Citadel Development Foundation. A complex coding system was used in the original file to indicate upper and lower case letters in the intensity field, blended lines (* in intensity field), changes from Catalaen et al. (1964) in combination with other codes, and other combinations of individual codes. The format and coding system were extensively revised by W. H. Warren Jr. at the Astronomical Data Center in order to prepare a uniform file fully processable by machine, to replace all upper case characters by lower case where appropriate, to insert parentheses and asterisks, and to duplicate the format used in an earlier finding list for the NSRDS-NBS3 multiplet tables prepared by Adelman et al. (1985) to the extent possible. The complete table was sorted various ways to detect errors and was proofread in sections by S. J. Adelman. The final multiplet-ordered table was sorted by computer to produce the wavelength-ordered table. The original Script file was translated to ASCII and put into the current standard from by the undersigned. VI_34.xml Annotated Bibliography of Multivariate Statistical Methods in Astronomy 6037 VI/37 Bibliography of Statistical Methods in Astronomy Annotated Bibliography of Multivariate Statistical Methods in Astronomy F Murtagh A Heck Astron. Astrophys. Suppl. Ser. 68 113 1987 1987A&AS...68..113M Bibliography This catalog contains a bibliography of statistical data analysis and pattern recognition algorithms that are multivariate. References to computer packages and books are given. The catalog is divided into nine sections, each with astronomical and general headings, and is offered in two versions, LaTeX and ASCII.
bib.txt ASCII version of bibliography bib.tex LaTeX version of bibliography N. G. Roman ADC/SSDOO 1997 Jul 25 VI_37.xml Model Atmospheres for G, F, A, B, and O Stars 6039 VI/39 Model Atmospheres for G,F,A,B,O Stars Model Atmospheres for G, F, A, B, and O Stars R L Kurucz Astrophys. Journ. Suppl. 40 1 1979 1979ApJS...40....1K Models, atmosphere This catalog lists fluxes and temperature-mass relations for 1200 models. The first 284 models are from Kurucz, R.L., Ap.J. Supp., 40, 1, 1979. Next 325 models are purely radiative models for A and B stars with Teff 8000K to 20000K for the metallicity/hydrogen abundance ratios (in log10 scale), [M/H] = -1., -.5, +.5, +1. Finally the last 591 models are new improved convective models for 5500K to 8500K with [M/H]= +1., +.5,0., -.5, -1., -1.5, -2., -2.5, -3., -9.99. Because the new models have not yet been published and because Dr. Kurucz is computing visible and infrared colors in various photometric systems, these new fluxes should not be used to publish colors without his agreement (Kurucz 1993, private communications). The data in this catalog are very outdated. Dr. Kurucz is sending the ADC an updated version while he works on an up-to-date version. He has an extensive amount of data available and distributes them on CD-ROM. Email kurucz@cfa.harvard.edu for details.
Summary of model parameters Model Model number, 1 - 1200 --- Teff Effective temperature K log.g Surface gravity cm/s2 log.Ab Abundance Sun note.tex Note about units cdrom.txt List of CD-ROMs available from Dr. Kurucz C.-H. Joseph Lyu Hughes STX/NASA 1996 Aug 22 There was no previous ADC documentation and a brief description (Intro) by CDS (1993) was used to create this ReadMe file. UNKNOWN UNKNOWN To retrieve information from the original data file 'main' easier, we split this 'main' file into two tables, table4.dat and table6.dat. They contain similar data columns as tables 4 and 6 of Kurucz (1979), respectively. And we create two standard Fortran codes to read these catalog data files. See the enclosed note.tex (standard latex) for units in table6.dat. A file (grid), models, which contains the basic parameters of the the 1200 models has been directly created from the catalog data files. VI_39.xml The Revised Yale Isochrones and Luminosity Functions 6040 VI/40 Revised Yale Isochrones and Luminosity Functions The Revised Yale Isochrones and Luminosity Functions E M Green P Demarque C R King Yale University Observatory, New Haven, Connecticut ??? ??? 1987 1987ryil.book.....G Models, evolutionary Isochrones Stars, ages The revised isochrones and luminosity functions (LFs) are based on the stellar evolution calculations of Mengel et al. (1979) and Sweigart and Gross (1978). The revised tables comprise the most complete (as of 1987) isochrone grid available in both age and composition. The improvement in the revised catalog is the inclusion of UBVRI data as well as the theoretical quantities, which are empirically matched to a wide range of observational UBVRI data (Green et al. 1987, unpublished). These tables enable users to interpolate between isochrones, to plot isochrones in order to fit color-magnitude diagrams, luminosity functions to compare with observational data, and to construct stellar population models. To facilitate the use of isochrones, we (at the Astronomical Data Center, in 1987) had made available several FORTRAN programs, ISOTRP, LF, and subroutines. They incorporate our experience of the best methods of interpolation, minimization of precision problems, and how to deal with compositions and ages that are not always complete. ISOTRP allows the user to interpolate for any helium abundance or metallicity in the range of the Revised Yale Isochrone tables. LF constructs customized differential luminosity functions for Mbol or a UBVRI magnitude, for any bin size, and for any initial mass functions. In addition to the 24 isochrone files and the FORTRAN programs, we (at ADC) have included the color table that was used to convert from [Fe/H], log Teff, and log g to BC, U-B, B-V, V-R, R-I, in the isochrone data files. The data cover a complete grid with [Fe/H] from 1.00 to -3.5 in steps of 0.50, Teff from 2800 to 20000 K, and log g from 0.00 to 6.00.
The isochrone header file Name Isochrone filename --- IGB Evolutionary status 0 indicates Main Sequence (MS) turnoff only -1 means Red Giant branch (RGB) included --- Num Number of points for this isochrone --- Alpha Mixing length to scale height ratio Effective convective mixing length to pressure scale height ratio, always 1.50. --- The isochrones for Z=1E-1 and Y=0.20 The isochrones for Z=1E-1 and Y=0.30 The isochrones for Z=1E-2 and Y=0.10 The isochrones for Z=1E-2 and Y=0.20 The isochrones for Z=1E-2 and Y=0.30 The isochrones for Z=1E-2 and Y=0.40 The isochrones for Z=1E-3 and Y=0.10 The isochrones for Z=1E-3 and Y=0.20 The isochrones for Z=1E-3 and Y=0.30 The isochrones for Z=1E-3 and Y=0.40 The isochrones for Z=1E-4 and Y=0.10 The isochrones for Z=1E-4 and Y=0.20 The isochrones for Z=1E-4 and Y=0.30 The isochrones for Z=1E-4 and Y=0.40 The isochrones for Z=1E-5 and Y=0.10 The isochrones for Z=1E-5 and Y=0.20 The isochrones for Z=1E-5 and Y=0.30 The isochrones for Z=1E-5 and Y=0.40 The isochrones for Z=4E-2 and Y=0.20 The isochrones for Z=4E-2 and Y=0.30 The isochrones for Z=4E-3 and Y=0.20 The isochrones for Z=4E-3 and Y=0.30 The isochrones for Z=4E-4 and Y=0.20 The isochrones for Z=4E-4 and Y=0.30 EEP Equivalent evolutionary point number --- Mflag Mass data flag "*" if the mass point was extrapolated or it was interpolated over a very large interval. --- AGE The age in units of 10^6 yrs Myr Y Helium abundance % Z Metal abundance Metal abundance. The only exceptions are that Z = 0000 then Z is 1 and if Z = 9999 then Z is 10000 (in units of 1E-5) 10-5 Mass Mass solMass Teff Effective temperature K Lumin Luminosity solLum DN1 Initial mass function 1 The number of stars between J and J+1, for three different MS initial mass functions, s=1+x=0, 2.35, and 4.00, where dN(m) =~ m^(-s). The constant s was chosen to normalize all dN to 1000 stars in the range 0.5 < m < 1.0 solar masses on the initial MS. --- DN2 Initial mass function 2 --- DN3 Initial mass function 3 --- V Visual magnitude UBVRI magnitude and colors; Johnson UBV and Cousins RI. About the isochrone files: Each isochrone file contains isochrones for a single composition. The first 2 numbers of the file extension indicate Z, and the third number indicates Y for that file. For example iso123.dat contains data for Z=1x10^(-2), Y=0.30; iso432.dat pertains to Z=4x10-3, Y=0.20, etc. Zsun has been defined to be 0.02. Each isochrone file has a Zero Age Main Sequence (ZAMS) plus as many of the following ages as could be interpolated (or reasonably extrapolated) from the Mengel et al. (1979) and Sweigart and Gross (1978) mass tracks (units are 10 yrs): 150, 200, 350, 500, 750, 1000, 1500, 2000, 3000, 4000, 5000, 6000, 7000, 8000, 9000, 10000, 11000, 12000, 13000, 14000, 15000, 16000, 17000, 18000, 20000, 22000, 25000. The data files include the following compositions and ages: Z Y MS-turnoff ages Age range with Giant-Branches ------------------------------------------------------------ 0.00001 0.10 0, 200 - 25000 none 0.20 0, 200 - 25000 11000 - 25000 0.30 0, 150 - 25000 6000 - 25000 0.40 0, 150 - 18000 none ------------------------------------------------------------ 0.0001 0.10 0, 200 - 25000 none 0.20 0, 200 - 25000 3000 - 25000 0.30 0, 150 - 25000 6000 - 25000 0.40 0, 200 - 18000 none ------------------------------------------------------------ 0.0004 0.20 0, 200 - 25000 3000 - 25000 0.30 0, 150 - 25000 6000 - 20000 ------------------------------------------------------------ 0.001 0.10 0, 200 - 25000 none 0.20 0, 200 - 25000 6000 - 25000 0.30 0, 150 - 25000 7000 - 25000 0.40 0, 150 - 18000 none ------------------------------------------------------------ 0.004 0.20 0, 200 - 25000 3000 - 22000 0.30 0, 150 - 17000 6000 - 17000 ------------------------------------------------------------ 0.01 0.10 0, 200 - 25000 15000 - 25000 0.20 0, 150 - 2500 750 - 25000 0.30 0, 150 - 20000 500 - 20000 0.40 0, 150 - 20000 3000 - 20000 ------------------------------------------------------------ 0.04 0.20 0, 150 - 22000 3000 - 22000 0.30 0, 150 - 25000 1500 - 25000 ------------------------------------------------------------ 0.1 0.20 0, 150 - 22000 none 0.30 0, 150 - 25000 none ------------------------------------------------------------ mag U-B Photoelectric U-B colors mag B-V Photoelectric B-V colors mag V-R Photoelectric V-R colors mag R-I Photoelectric R-I colors mag Color Table FeHratio The abundance ratio of Fe and H --- Teff Gas effective temperature K Log(g) Log of gravity cm/s2 BC Bolometric Corrections mag U-B Photoelectric U-B colors mag B-V Photoelectric B-V colors mag V-R Photoelectric V-R colors mag R-I Photoelectric R-I colors mag C.-H. Joseph Lyu, Paul Kuin Hughes STX/NASA 1996 Jul 12 The original introductory text of "The Revised Yale Isochrones and Luminosity Functions" by Green et al. (1987) and its attached letter of Wayne H. Warren were used to create this ReadMe file. The author provided the color calibration reference. VI_40.xml Identification of a Constellation from a Position 6042 VI/42 Identification of a Constellation From Position Identification of a Constellation from a Position N G Roman Pub. Astron. Soc. Pac. 99 695 1987 1987PASP...99..695R Constellations A table of constellation boundaries was rearranged to permit the rapid identification of the constellation to which a position refers. A software program is provided to precess positions at another equinox to those at 1875.0.
Barry Rappaport put the list of constellation boundaries that was published in 1930 (Delporte 1930) into electronic form. This form made it convenient to manipulate the data into an arrangement that is easier to use for finding a constellation from a position. The southern boundaries of each constellation are listed in order of declination and then by the eastern terminus of each declination arc. A program, in FORTRAN77, for determining the constellation using the data in data.dat is provided in two forms. Comments describe the format in which the positions must be entered. The main program is followed by a precession subroutine which permits the use of positions at any epoch. The file data.dat is a list of constellation boundaries in the form Lower Right Ascension, Upper Right Ascension, Lower Declination, three letter abbreviation for the Constellation. The following is an example of the output of the program: RA = 9.0000 DEC = 65.0000 IS IN CONSTELLATION UMa RA = 23.5000 DEC = -20.0000 IS IN CONSTELLATION Aqr RA = 5.1200 DEC = 9.1200 IS IN CONSTELLATION Ori RA = 9.4555 DEC = -19.9000 IS IN CONSTELLATION Hya RA = 12.8888 DEC = 22.0000 IS IN CONSTELLATION Com RA = 15.6687 DEC = -12.1234 IS IN CONSTELLATION Lib RA = 19.0000 DEC = -40.0000 IS IN CONSTELLATION CrA RA = 6.2222 DEC = -81.1234 IS IN CONSTELLATION Men END OF INPUT POSITIONS AFTER: RA = 6.2222 DEC = -81.1234 THE EQUINOX FOR THESE POSITIONS IS 1950.0 A C version of the program for those who have not access to a f77 compiler is also available.
The data file with constellation boundaries RA_low Lower right ascension range, equinox=1875 h RA_up Upper right ascension range, equinox=1875 h DE_up Upper declination, equinox=1875 deg const Constellation name --- Nancy Grace Roman ADC/SSDOO 1996 Feb 22 VI_42.xml A Finding List for Observers of Interacting Binary Systems, 5th Edition 6044 VI/44 Finding List of Interacting Binaries, 5th ed. A Finding List for Observers of Interacting Binary Systems, 5th Edition F B Wood J P Oliver D R Florkowski R H Koch Publ. Dept. of Astron., Univ. of Florida, Vol. I ??? ??? 1980 1980floi.book.....W Binaries, eclipsing Binaries, orbits Binaries, spectroscopic Finding lists Stars, double and multiple This catalog is abstracted from the Card Catalog maintained at the University of Florida containing information on all published, and to the extent available, unpublished work on eclipsing binaries. The fifth edition differs from the previous ones in the extension of the magnitude limit at maximum light from 13 to 15. The catalog fields are Finding List number; star name; position (equinox 1900); blue magnitude at maximum light; bandpass of maximum light; depth of primary minimum in same bandpass; bandpass primary minimum; depth of secondary minimum and its bandpass; spectral class of star eclipsed at primary light and optional uncertainty character; spectral class of star eclipsed at secondary light; most recent reliable epoch of primary minimum; most recent orbital period; duration of primary minimum; duration of totality of primary minimum; BD, CoD, CPD, and HD number; alternate designations of system; codes indicating the nature of the system.
The Finding List of Interacting Binaires Seq Finding List Number. --- Name Name of star --- RAh Right Ascension 1900 (hours) h RAm Right Ascension 1900 (minutes) min DE- Declination 1900 (sign) --- DEd Declination 1900 (degrees) deg Bmax Blue (or other, see n_Bmax) magnitude at maximum light. mag n_Bmax Bandpass or note for Bmax number=1 this field indicates the bandpass if not B (V=visible, I=infrared, U=ultraviolet), a colon (:) for bandpass uncertainty, or a N for a note (file "remarks") --- Depth1 Depth of primary minimum light. mag n_Depth1 Bandpass or note for Depth1 number=1 this field indicates the bandpass if not B (V=visible, I=infrared, U=ultraviolet), a colon (:) for bandpass uncertainty, or a N for a note (file "remarks") --- Depth2 Depth of secondary minimum mag n_Depth2 Bandpass or note for Depth2 number=1 this field indicates the bandpass if not B (V=visible, I=infrared, U=ultraviolet), a colon (:) for bandpass uncertainty, or a N for a note (file "remarks") --- Sp1 Spectral class of primary. number=2 the colon (:) means "uncertain", and the question mark (?) means "very uncertain" --- n_Sp1 N=note about spectral class. --- Sp2 Spectral class of secondary. number=2 the colon (:) means "uncertain", and the question mark (?) means "very uncertain" --- n_Sp2 N=note about spectral class. --- Ep1 Most recent epoch of primary minimum (JD) d n_Ep1 N=note about epoch. :=epoch uncertainty. --- Period Most recent Orbital period, in days or years (see n_Period). d n_Period Y=Period expressed in year number=3 'N' indicates a note, and the colon (:) means "uncertain" --- min1Dur =-999 Duration of primary minimum, in hours, days or years (see n_min1Dur) h n_min1Dur Unit of duration, D=days, Y=years. See also note number=2 the colon (:) means "uncertain", and the question mark (?) means "very uncertain" --- totDur =-999 Duration of totality. in hours, days or years (see n_totDur) h n_totDur Unit of totality, D=days, Y=years. See also note number=2 the colon (:) means "uncertain", and the question mark (?) means "very uncertain" --- BD Bonner Durchmusterung (BD) number. --- CD Cordoba Durchmusterung (CD) number. --- CPD Cape Photographic Durchmusterung (CPD) number. --- HD The Henry Draper Catalog (HD) number. --- Names Alternate designations --- --- Coded remarks system number=4 the following 1-letter codes are used: A variable period B variable period? C light elements uncertain D eccentric orbit E faint companion F third light G times of minimum recorded by group such as AAVSO, BBSAG, etc. H variable comparison star? J atmospheric eclipses K asymmetric light curve L variable light curve M light curve poorly known N asymmetric minima P photometric analysis available Q hydrogen emission seen R Ca II emission seen S radial velocity curve available T variable radial velocity curve U double-lined spectroscopic binary V absolute dimension known W UV excess X IR excess Y polarization observed Z variable polarization 1 X-ray source 2 radio source 3 visual binary 4 cluster member 5 intrinsic variable 6 ellipsoidal variable 7 not eclipsing binary? 8 apsidal motion --- Remarks for designated systems. Seq Finding List Number. --- Name Star name, as in "catalog" --- Text Text of notes number=1 If the notes are longer than 120 bytes, they start from the 15th byte of next logical record until they end, while Seq and star name are repeated in the fields of 1-4 bytes and 5-13 bytes respectively. --- adc.doc Original ADC documentation, by Young Woon Kang (see "Historical Notes" section) Gail L. Schneider SSDOO/ADC Francois Ochsenbein CDS 1996 Jan 04 UNKNOWN UNKNOWN Previous editions: Koch, R. H., Sobieski S., and Wood, F. B. 1963, A Finding List for Observers of Eclipsing Variables, 4th edition, University of Pennsylvania Astronomical Series, Vol. IX. Wood, F. B. 1953, A Finding List for Observers of Eclipsing Variables, 3rd edition, University of Pennsylvania Astronomical Series, Vol. VIII. Pierce, N. L. 1947, A Finding List for Observers of Eclipsing Variables, 2nd edition, Princeton University Observatory Contribution No. 22. * The machine version was received from the authors in March 1981, processed and documented by Young Woon Kang at ADC: see Section 4 of the "adc.doc" file. * January 1996: the documentation was standardized at CDS; in this process, a few misalignments and corrections was made at CDS for Seq: 311 (in Epoch1) 767 (in Depth1) 876 (removed 'D' in n_Period column) 1549 (replaced blank min1Dur by -999) 1551 (replaced blank min1Dur by -999) 1596 (replaced blank min1Dur by -999) 2425 (in Depth1) 2766 (removed trailing 0 in Depth2) 3228 (in min1Dur) VI_44.xml Fe II Reference Catalogue 6048 VI/48 Fe II Reference Catalogue Fe II Reference Catalogue R Viotti G B Baratta Astron. Astrophys. Suppl. Ser. 75 497 1988 1988A&AS...75..497V Fe II Reference Catalogue R Viotti A Vittone M Friedjung Solar Physics 120 209 1989 1989SoPh..120..209V Atomic physics Bibliography In order to give a ground for current works on the physics of formation of lines of FeII and of other similar ions in the spectra of astrophysical objects, an extensive Catalogue of all the articles published on the matter until June 1986 is given. Many articles published after that date are also included in the Catalogue. All the articles are arranged in three tables by alphabetical and chronological order, by physical subject and by astro- physical category.
The FeII Problem has since long attracted the interest of many researchers. Lines of singly ionized iron are present in absorption or in emission in the spectrum of many different categories of astrophysical objects, from the Sun, to early and late stars, diffuse nebulae and distant galaxies. Their presence is frequently an evidence of non thermal equilibrium phenomena. A large number of works have been so far devoted to the study of the FeII problem, although many of the oldest ones are only of historical interest. In recent years, the beginning of the space ultraviolet era, the rapid development of new observational techniques, as well as the new laboratory works on FeII and the extensive use of large computers for theoretical re- search, has stimulated a renewed interest in the field and the number of current works is rapidly increasing. Recently, an entire IAU Colloquium was organized on the "Physics of Formation of FeII Lines Outside LTE" (Viotti et al. 1988). The aim of this Catalogue is to collect all, or nearly all, the titles of the articles related to the problem of FeII line formation and to the basic physics concerned the problem. The Catalogue in its earlier version (Viotti and Baratta 1988) included all the articles published until June 1986, i.e. before the IAU Colloquium No.94 held in Capri, on the occasion of which this work has been undertaken. This is an updated version which also includes more recent articles.
Bibliography with full references text Text of references Full references to articles are arranged in alphabetical (by author) and chronological order. Keywords from the subject and category lists (see notes for subindex.dat) are included after each reference. --- Concise references by subject and category text Text of subject keyword index References to articles are arranged by physical subject (beginning with record 4), and by astrophysical categories (beginning with record 443). The following subjects and categories have been considered. (Note that for practical reasons, round brackets instead of square brackets were used to indicate forbidden transitions.) Subjects: - Atomic data (levels, gf-values, collision strengths, etc.) - Physical processes (excitation, including selective excitation processes, ionization and recombination) - Data analysis (excitation temperature, curve of growth, self absorption curves) - Model (theoretical models of the line formation region) - Spectral synthesis - Observation of FeII, (FeII) lines: - line identification - line intensity - line profiles, including broad emission - (FeII) absorption lines - Other atomic species (FeI, FeIII to FeVII, Co, Ni, etc.) - General (review articles, catalogues, surveys) Astrophysical Categories: - The Sun (photosphere, chromosphere) - Stars, late (G-type or later, T Tau and Mira variables, etc.) - Stars, early (F-type or earlier, Ae, Be) - Stars, Luminous Blue Variables (LBV = P Cyg, S Dor, Hubble-Sandage variables) - Stars, variables (binaries, symbiotic stars,VV Cep and R CrB variables, novae) - Diffuse matter (Herbig-Haro objects, supernovae, SNR, diffuse nebulae, interstellar matter) - Extragalactic astronomy (normal galaxies, active galactic nuclei). --- Julie Anne Watko SSDOO/ADC 1996 Jun 20 Documentation for this catalogue was originally prepared by Roberto Viotti of the Istituto Astrofisica Spaziale, (CNR, Via Enrico Fermi 21, C. P. 67, I 00044 Frascati (RM), Italy) and Giovanni Battista Baratta of the Osser- vatorio Astronomico, (Via del Parco Mellini 84, I 00161 Roma, Italy). Much of the text of this ReadMe file is taken verbatim from their document. The original authors are indebted to many persons for useful suggestions on the compilation of this Catalogue. Thanks are in particular due to M. Friedjung, S. Johansson, M. Joly, C. Jordan, and J.P. Swings. These authors would appreciate having brought to their attention any error and omission noted in this Catalogue. VI_48.xml Collisional Excitation of Formaldehyde in "Hot" Interstellar Molecular Regions 6051 VI/51 Collisional Excitation Rates of Formaldehyde Collisional Excitation of Formaldehyde in "Hot" Interstellar Molecular Regions S Green Astrophys. J. Suppl. Ser. 76 979 1991 1991ApJS...76..979G Excitation rates Interstellar medium Earlier calculations for rotational excitation of formaldehyde H2CO collisions with He atoms are extended to include the 81 lowest rotational levels and kinetic temperatures to 300K.
Rotational Levels for ortho-H2CO Rotational Levels for para-H2CO Level Rotational level number --- J quantum number --- K quantum number --- Parity --- E Rotational energy cm-1 Rate constants for ortho-H2CO (Table 3) Rate constants for para-H2CO (Table 2) i Initial H2CO rotor level --- f Final H2CO rotor level --- R10 Rate constant, temperature 10K cm3/s R15 Rate constant, temperature 15 cm3/s R20 Rate constant, temperature 20 cm3/s R30 Rate constant, temperature 30K cm3/s R40 Rate constant, temperature 40K cm3/s R50 Rate constant, temperature 50K cm3/s R60 Rate constant, temperature 60K cm3/s R70 Rate constant, temperature 70K cm3/s R80 Rate constant, temperature 80K cm3/s R90 Rate constant, temperature 90K cm3/s R100 Rate constant, temperature 100K cm3/s R120 Rate constant, temperature 120K cm3/s R140 Rate constant, temperature 140K cm3/s R160 Rate constant, temperature 160K cm3/s R180 Rate constant, temperature 180K cm3/s R200 Rate constant, temperature 200K cm3/s R220 Rate constant, temperature 220K cm3/s R240 Rate constant, temperature 240K cm3/s R260 Rate constant, temperature 260K cm3/s R280 Rate constant, temperature 280K cm3/s R300 Rate constant, temperature 300K cm3/s Francois Ochsenbein CDS 1994 Feb 03 VI_51.xml Horizontal Branch Stellar Model Calculations 6054 VI/54 Horizontal Branch Stellar Model Calculations Horizontal Branch Stellar Model Calculations B Dorman Astrophys. J. Suppl. Ser. 81 221 1992 1992ApJS...81..221D Abundances, [Fe/H] Isochrones Stars, horizontal branch This data set consists of evolutionary sequences from the Zero Age Horizontal Branch (ZAHB) to the point where log L/Lsun reaches 2.25 on the lower AGB. These calculations have enhanced oxygen abundance according to a relation used by VandenBerg (1992ApJ...391..685V) and Bergbusch and VandenBerg (1992ApJS...81..163B) for main sequence and red-giant branch models. Also, zero age sequences for oxygen enhanced and scaled-solar compositions are given.
There are thirteen data files in this directory, ten of which contain evolutionary sequences from the ZAHB to the point where log(L/Lsun) reaches 2.25 on the lower AGB. These calculations have enhanced oxygen abundance according to a relation used by VandenBerg (1992) and Bergbusch and VandenBerg (1992) in computations of evolutionary tracks and isochrones for main sequence and red-giant branch models. The other three contain zero age sequences for oxygen enhanced and scaled-solar compositions, as explained below. The models with [O/Fe]>0 are described in more detail in Dorman (1992). Briefly, the models use Los Alamos (1977) high temperature opacities, Alexander (1980) low temperature opacities, the reaction rates listed in Caughlan and Fowler (1988), and the Eggleton et. al. (1973) equation of state. model atmospheres for surface pressures used by VandenBerg (1992), and a mixing length of 1.5 pressure scale heights. Accompanying scaled-solar evolution calculations may be available on request, through the address given below. A complete bibliography for the input physics in these models can be found from the 3 papers listed in the References below. Evolutionary sequences: The ten files are for ten different compositions, lying between [Fe/H]=-2.26 and -0.47. The filenames (f24a14.dat,f24b24.dat etc.) are significant in the sense that the `24' which appears in every name refers to the ZAMS helium abundance, to two significant figures. The `14', `24', `34' etc. gives the mantissa and exponent of the value of Z', the heavy element abundance of a model with the same [Fe/H], but without the oxygen enhancement. Thus, f24j63.dat contains sequences with the same iron abundance as scaled solar models with Z = 0.006. A summary of the contents of each file is given below. The tables here have been derived from the original calculations using cubic Hermite spline interpolation, and are tabulated at even intervals of the central helium abundances; the intervals change towards exhaustion. After Y is exhausted at the centre of the model, the tracks are tabulated at intervals of 0.25 Myr. ---------------------------------------------- Filename YHB [Fe/H] [O/Fe] Msh ---------------------------------------------- f24a14.dat 0.246 -2.26 0.75 0.4926 f24b24.dat 0.247 -2.03 0.70 0.4904 f24c34.dat 0.248 -1.78 0.66 0.4881 f24d44.dat 0.248 -1.66 0.63 0.4866 f24e64.dat 0.249 -1.48 0.60 0.4852 f24f13.dat 0.250 -1.26 0.55 0.4835 f24g23.dat 0.252 -1.03 0.50 0.4815 f24h33.dat 0.257 -0.78 0.39 0.4792 f24i43.dat 0.259 -0.65 0.30 0.4776 f24j63.dat 0.266 -0.47 0.23 0.4757 ---------------------------------------------- Zero Age Horizontal Branch models: There is one file for [O/Fe] > 0 models (zahbo.dat), and there are two for scaled solar calculations. The first of these (zahb.dat) contains ZAHB models for the [Fe/H] values which correspond to the enhanced oxygen sets. The other (zahbs.dat), containing models for just 3 compositions, has data for [Fe/H] = -0.23, 0 and +0.15 ( Z = 0.01, 0.0169 and 0.024). These have been calculated with the Krishna-Swamy scaled-solar T-tau relation and with mixing length 1.58 pressure scaleheights. They are not consistent with the others, therefore, and using them together to derive theoretical quantities as a function of metallicity may give spurious results. All of the oxygen-enhanced ZAHBs contain models for masses between about 0.5 and 1.5 solar masses, while the range of the scaled-solar models varies.
Evolutionary sequence [Fe/H]=-2.26 Evolutionary sequence [Fe/H]=-2.03 Evolutionary sequence [Fe/H]=-1.78 Evolutionary sequence [Fe/H]=-1.66 Evolutionary sequence [Fe/H]=-1.48 Evolutionary sequence [Fe/H]=-1.26 Evolutionary sequence [Fe/H]=-1.03 Evolutionary sequence [Fe/H]=-0.78 Evolutionary sequence [Fe/H]=-0.65 Evolutionary sequence [Fe/H]=-0.47 Mass Stellar mass solMass [Fe/H] Metallicity relative to Sun (log scale) Sun [O/Fe] Oxygen abundance relative to Sun (log scale) Sun Age Age in Myr since ZAHB Myr Yc Central helium fraction --- logL Surface luminosity (log scale) solLum logTe Effective temperature (log scale) K log.g Surface gravity, cgs units (log scale) cm/s2 Mv Absolute Visual magnitude, derived from scale described by VandenBerg (1992ApJ...391..685V) mag B-V colour index mag logTc Central Temperature (log scale) K log.rho_c Central density, cgs units (log scale) g/cm3 Mccore Mass of convective core solMass Mout Mass at outer edge of semiconvection zone solMass Msh Mass at peak energy production rate of Hydrogen burning shell solMass A A = log.L/M^0.81, a quantity arising from pulsation models number=1 the two quantities A and logP are given for 3.79 < log T < 3.90. --- logP Period of RR Lyrae pulsation (log scale) in the fundamental mode number=1 the two quantities A and logP are given for 3.79 < log T < 3.90. d Zero Age Horizontal Branch model. Scaled solar sequences Zero Age Horizontal Branch model. Enhanced O ZAHB Sequences Zero Age Horizontal Branch model. Scaled solar metal rich compositions YHB Helium abundance --- [Fe/H] Metallicity relative to Sun (log scale) Sun [O/Fe] Oxygen abundance relative to Sun (log scale) Sun Msh Core mass at He flash solMass Mass Stellar mass (solar units) solMass logL Surface luminosity (log scale) solLum logTe Effective temperature (log scale) K log.g Surface gravity, cgs units (log scale) cm/s2 Mv Absolute Visual magnitude mag B-V colour index mag logR Radius (log scale) cm logTc Central Temperature (log scale) K log.rho_c Central density, cgs units (log scale) g/cm3 CDS Catalogue Service CDS 1996 Mar 04 We thank Ben Dorman <bd4r@borealis.astro.Virginia.EDU> for providing the files and the necessary explanations in early 1992. VI_54.xml Evolution of 0.7-3.0 M stars having -1.0 <= Fe/H 0.0 6055 VI/55 Evolutionary Tracks and Isochrones Evolution of 0.7-3.0 M stars having -1.0 <= Fe/H 0.0 D A VandenBerg Astrophys. J. Suppl. Ser. 58 711 1985 1985ApJS...58..711V Evolution of 0.7-3.0 M stars having -1.0 <= Fe/H 0.0 D A VandenBerg R A Bell Astrophys. J. Suppl. Ser. 58 561 1985 1985ApJS...58..561V Evolution of 0.7-3.0 M stars having -1.0 <= Fe/H 0.0 R A Bell D A VandenBerg Astrophys. J. Suppl. Ser. 63 335 1987 1987ApJS...63..335B Evolution of 0.7-3.0 M stars having -1.0 <= Fe/H 0.0 D A VandenBerg P G Laskarides Astrophys. J. Suppl. Ser. 64 103 1987 1987ApJS...64..103V Evolution of 0.7-3.0 M stars having -1.0 <= Fe/H 0.0 C R Proffitt D A VandenBerg Astrophys. J. Suppl. Ser. 77 473 1991 1991ApJS...77..473P Evolution of 0.7-3.0 M stars having -1.0 <= Fe/H 0.0 D A VandenBerg Astrophys. J. 391 685 1992 1992ApJ...391..685V Evolution of 0.7-3.0 M stars having -1.0 <= Fe/H 0.0 P A Bergbusch D A VandenBerg Astrophys. J. Suppl. Ser. 81 163 1992 1992ApJS...81..163B Isochrones The following data and program files are provided: 1. Evolutionary tracks/isochrones from VandenBerg (1985, ApJS, 58, 711): "Evolution of 0.7-3.0 Solar masses stars having -1.0<=[Fe/H]<=0.0" V852M3.TRK and V852M3.ISO - Y=0.25, Z=0.0017 V853M3.TRK and V853M3.ISO - Y=0.25, Z=0.0030 V856M3.TRK and V856M3.ISO - Y=0.25, Z=0.0060 V851M2.TRK and V851M2.ISO - Y=0.25, Z=0.0100 V852M2.TRK and V852M2.ISO - Y=0.25, Z=0.0169 Note that 'V852M3' represents 'V(andenBerg 19)85' results for a metal abundance '2 (times 10 to the) M(inus) 3'. That is, the file name gives the initials of the author(s), the year of publication, and the assumed value of Z (the mass-fraction metal abundance) to one significant figure. This convention is used for all data files in this package. Reference should be made to V85 to assist the identification of the quantities that are contained in the files. Note that, in the case of the above .ISO files, a zero-age main sequence is given as well as isochrones for ages from 0.3 to 15 Gyr. 2. Isochrones from VandenBerg & Bell (1985, ApJS, 58, 561) and Bell & "Theoretical isochrones for Globular Clusters" VandenBerg (1987, ApJS, 63, 335): VB851M4A.ISO and VB851M4B.ISO - Z=0.0001 (Y=0.2 & Y=0.3) VB853M4A.ISO and VB853M4B.ISO - Z=0.0003 (Y=0.2 & Y=0.3) VB851M3A.ISO and VB851M3B.ISO - Z=0.0010 (Y=0.2 & Y=0.3) VB853M3A.ISO and VB853M3B.ISO - Z=0.0030 (Y=0.2 & Y=0.3) VB856M3A.ISO and VB856M3B.ISO - Z=0.0060 (Y=0.2 & Y=0.3) Note that 'A' or 'B' has been appended to the file name to indicate Y=0.2 or Y=0.3, respectively. (The file name has been limited to 8 characters so as not to exceed the maximum length permitted on IBM machines.) Once again, reference should be made to the two published papers to identify the quantities that have been saved. 3. Evolutionary tracks/isochrones from VandenBerg & Laskarides (1987, ApJS, 64, 103): "Theoretical isochrones for old, super-metal-rich stars" VL873M2A.TRK and VL873M2A.ISO - Y=0.25, Z=0.03 VL873M2B.TRK and VL873M2B.ISO - Y=0.35, Z=0.03 VL876M2A.TRK and VL876M2A.ISO - Y=0.25, Z=0.06 VL876M2B.TRK and VL876M2B.ISO - Y=0.35, Z=0.06 VL871M1A.TRK and VL871M1A.ISO - Y=0.25, Z=0.10 VL871M1B.TRK and VL871M1B.ISO - Y=0.35, Z=0.10 Note that 'A' or 'B' has been appended to the file name to indicate Y=0.25 or Y=0.35, respectively. The .TRK files are self-explanatory; in the case of the .ISO files, each line gives 'mass, Mbol, and log Teff' values for each of three consecutive points along an isochrone. No attempt has been made to transform the models to the observed plane 4. Isochrones from Proffitt & VandenBerg (1991, ApJS 77, 473): "Implication of He diffusion for globular cluster isochrones and luminosity functions": PV911M4S.ISO and PV911M4D.ISO - Z=0.0001 (without/with diffusion) PV911M3S.ISO and PV911M3D.ISO - Z=0.0010 (without/with diffusion) PV914M3S.ISO and PV914M3D.ISO - Z=0.0040 (without/with diffusion) Note that 'S' and 'D' have been appended to the file name to indicate 'standard' or 'diffusive' calculation, respectively. The Z values given above refer to the mass-fraction of metals exclusive of the assumed oxygen abundance enhancement. (See point 6. below) 5. Isochrones from Bergbusch & VandenBerg (1992, ApJS 81, 163) "Oxygen-enhanced models for globular cluster stars. II. Isochrones and luminosity functions" BV921M4.ISO - Z=0.0001 BV922M4.ISO - Z=0.00017 BV923M4.ISO - Z=0.0003 BV924M4.ISO - Z=0.0004 BV926M4.ISO - Z=0.0006 BV921M3.ISO - Z=0.0010 BV922M3.ISO - Z=0.0017 BV923M3.ISO - Z=0.0030 BV924M3.ISO - Z=0.0040 BV926M3.ISO - Z=0.0060 Note that the Z values given above refer to the mass-fraction of metals exclusive of the assumed oxygen abundance enhancement. 6. The luminosity function code (LUMVAX.FOR or LUMIBM.FOR): The names specify either a VAX or an IBM version of the code which can process any of the files in 4. or 5. above to produce tables of isochrones and luminosity functions. The tables which are generated should be identical to the tables that appear in the Proffitt & VandenBerg and the Bergbusch & VandenBerg studies. The first several lines in the two codes describe what is required to execute them. *** The tables can be generated as a set of files *.lf either on VAX (@make) or on Unix platforms (make) 7. COLLO.TXT and COLHI.TXT are the color transformation and bolometric correction data used to transpose the models from the theoretical to the observed plane. The user may wish to extract SUBROUTINE COLOR from LUMVAX.FOR or LUMIBM.FOR to derive colors for any [Fe/H] (preferably between 0.0 and -2.0), log g, and log Teff. Reference should be made to VandenBerg (1992, ApJ 391, 685) for a discussion of the transformation relations. Should the user encounter any difficulty with this package, he/she is invited to contact Don VandenBerg (davb@uvvm.uvic.ca).
Isochrones VandenBerg 1985 Y He composition --- Z Heavy elements composition --- Age Gyr Mass Sun logL Luminosity Sun log.Te Effective temperature K log.g Gravity cm/s2 Mbol Bolometric absolute magnitude mag Mv Visual absolute magnitude mag B-V Color index in Cousins system mag V-R Color index in Cousins system mag V-I Color index in Cousins system mag Evol.Tracks VandenBerg 1985 Y He composition --- Z Heavy elements composition --- Mass Mass Sun logL Luminosity Sun Mbol Bolometric absolute magnitude mag log.Te Effective temperature K log.g Gravity cm/s2 log.Tc Core temperature K log.rhoc Core density g/cm3 Age Gyr Mv Visual absolute magnitude mag B-V Color index in Cousins system mag V-I Color index in Cousins system mag V-R Color index in Cousins system mag Isochrones VandenBerg+Bell 1985 Y He composition --- Z Heavy elements composition --- Age Gyr Mass Sun logL Luminosity Sun log.Te Effective temperature K log.g Gravity cm/s2 Mbol Bolometric absolute magnitude mag M(V) Visual absolute magnitude mag B-V Color index in Cousins system mag R-I Color index in Cousins system mag V-R Color index in Cousins system mag b-y Color index in Stroemgren system mag c1 Color index in Stroemgren system mag m1 Color index in Stroemgren system mag u-b Color index in Stroemgren system mag c1E Color index in Eggen system mag m1E Color index in Eggen system mag u-v Color index in Thuan-Gunn system mag v-g Color index in Thuan-Gunn system mag g-r Color index in Thuan-Gunn system mag M(g) Absolute magnitude in Thuan-Gunn g filter mag M(R) Absolute magnitude in Cousins R filter mag M(y) Absolute magnitude in Stroemgren y filter mag Evol.Tracks VandenBerg+Laskarides 1987 Y He composition --- Z Heavy elements composition --- Mass Sun logL Luminosity Sun Mbol Bolometric absolute magnitude mag log.Te Effective temperature K log.g Gravity cm/s2 Log.Tc Core temperature K log.rhoc Core density g/cm3 Age Gyr Xc Fraction of H in core --- Msh Mass of the shell --- Isochrones VandenBerg+Laskarides 1987 Y He composition --- Z Heavy elements composition --- Age Gyr Mass Sun Mbol Bolometric absolute magnitude mag log.Te Effective temperature K Isochrones Proffitt+VandenBerg 1991 Isochrones Bergbusch+VandenBerg 1992 Y He composition number= The log.g value can be computed with log.g = log.Mass + 4.log.Te - logL - 10.6157 --- Z Heavy elements composition number= The log.g value can be computed with log.g = log.Mass + 4.log.Te - logL - 10.6157 --- [O/Fe] Oxygen abundance number= The log.g value can be computed with log.g = log.Mass + 4.log.Te - logL - 10.6157 Sun Diff Flag which takes the values: 's' for Standard Isochrones 'd' for Diffusion Isochrones number= The log.g value can be computed with log.g = log.Mass + 4.log.Te - logL - 10.6157 --- Age number= The log.g value can be computed with log.g = log.Mass + 4.log.Te - logL - 10.6157 Gyr Mass Mass number= The log.g value can be computed with log.g = log.Mass + 4.log.Te - logL - 10.6157 Sun logL Luminosity number= The log.g value can be computed with log.g = log.Mass + 4.log.Te - logL - 10.6157 Sun log.Te Effective temperature number= The log.g value can be computed with log.g = log.Mass + 4.log.Te - logL - 10.6157 K colhi.txt B-V and BC (high temperature) collo.txt B-V and BC (low temperature) Francois Ochsenbein CDS rev. Gail L. Schneider SSDOO/ADC 1998 Apr 03 Don VandenBerg <davb@uvvm.uvic.ca> UNKNOWN UNKNOWN * 15-Feb-1994: Makefile written at CDS First standardized document at CDS * 3-Apr-1998: Standardized document revisited at ADC VI_55.xml Tests of Shock Chemistry in IC 443G 6056 VI/56 Tests of shock chemistry in IC 443G Tests of Shock Chemistry in IC 443G B E Turner K -W Chan S Green D A Lubowich Astrophys. J. 399 114 1992 1992ApJ...399..114T Excitation rates The present study improves the computations of the collisional excitation rates by Green & Chapman (1978) for CS-H2; and by Bieniek & Green (1981) for SiO-H2. Part of the results are presented in the Appendix of the publication.
CS-H2 Collisional excitation rates SiO-H2 Collisional excitation rates Ji Initial rotational level --- Jf Final rotational level --- Rate(20) Collisional excitation rate at 20K cm3/s Rate(40) Collisional excitation rate at 40K cm3/s Rate(70) Collisional excitation rate at 70K cm3/s Rate(100) Collisional excitation rate at 100K cm3/s Rate(150) Collisional excitation rate at 150K cm3/s Rate(200) Collisional excitation rate at 200K cm3/s Rate(250) Collisional excitation rate at 250K cm3/s Rate(300) Collisional excitation rate at 300K cm3/s Francois Ochsenbein CDS 1994 Dec 13 UNKNOWN UNKNOWN by exchange from NASA-Goddard VI_56.xml High Resolution Absorption Cross Sections in the Transmission Window Region of the Schumann-Runge Bands and Herzberg Continuum of O2 6061 VI/61 O2 Absorption Cross Sections High Resolution Absorption Cross Sections in the Transmission Window Region of the Schumann-Runge Bands and Herzberg Continuum of O2 K Yoshino J R Esmond A S -C Cheung D E Freeman W H Parkinson Planetary Space Science, Vol. 40, No. 2/3, pp. 185-192, ??? ??? 1992 1992P&SS...40..185Y Atomic physics The absorption cross sections of the Schumann-Runge bands in the window region between the rotational lines have been measured in the wavelength region 180-195 nm. The measurements have been done with many different pressures of oxygen, 2.5-760 torr, so that the pressure- dependent absorption can be separated from the main cross sections. The published cross sections [Yoshino et al., Planet. Space Sci. 31, 339 (1983)] in the window region are superseded by the present cross sections. The combined cross sections are available at wavenumber intervals of ~0.1 cm-1. The Herzberg continuum cross sections are derived after subtracting calculated contributions from the Schumann-Runge bands and are significantly smaller than any previous measurements.
Data file (wave num 49362. - 50050.) Data file (wave num 50050. - 50720.) Data file (wave num 50720. - 51370.) Data file (wave num 50370. - 51980.) Data file (wave num 51980. - 52661.) Data file (wave num 52661. - 53250.) Data file (wave num 53250. - 53746.) Data file (wave num 53746. - 54256.) Data file (wave num 54260. - 54685.) Data file (wave num 54685. - 55115.) Data file (wave num 55115. - 55485.) Data file (wave num 55485. - 55800.) wavenum wave number in cm-1 cm-1 sigma Oxigen cross section/ molecule measured cm2 N. P.M. Kuin ADC/SSDOO/NASA 1995 Feb 13 Address of the authors: K. Yoshino, J.R. Esmond, A.S.-C. Cheung, D.E. Freeman and W.H. Parkinson Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, U.S.A. VI_61.xml Photoelectric absorption cross-sections with variable abundances 6062 VI/62 Photoelectric absorption cross-sections Photoelectric absorption cross-sections with variable abundances M Balucinska-Church D McCammon Astrophys. J. 400 699 1992 1992ApJ...400..699B Atomic physics Interstellar medium X-ray sources Polynomial fit coefficients have been obtained for the energy dependence of the photoelectric absorption cross sections of 17 astrophysically important elements. The aim of this work is to provide convenient fits to the photoelectric absorption cross sections for each of 17 elements separately, so that spectral modelling can be performed with an absorption term containing the abundances of some or all of the elements as adjustable parameters. The fits to the individual elements can also be used independently for calculating window transmissions, gas stopping efficiency, etc. The atomic absorption cross sections were taken from Henke et al. (1982). Polynomial fits have been made to the atomic absorption cross sections in the energy range of 0.03 -- 10 keV for seventeen elements: hydrogen, helium, carbon, nitrogen, oxygen, neon, sodium, magnesium, aluminium, silicon, sulphur, chlorine, argon, calcium, chromium, iron and nickel. In the case of elements with only the K-edge in this energy range, polynomial fits were made each side of the edge; with the L-edge also present three fits were made. Polynomials of up to degree 8 were required. The functions fit Henke's data points with a typical error of 2% and a maximum error of 7%, except for points below 40~eV for argon, calcium and sodium, where the errors are larger. The effective cross section per hydrogen atom for a particular set of elemental abundances may be simply calculated from the individual cross sections. A set of routines has been written in generic FORTRAN-77 to implement these polynomial fits. The file XSCTNS.FOR contains seventeen REAL functions that will return the photoelectric cross sections for H, He, C, N, O, Ne, Na, Mg, Al, Si, S, Cl, A, Ca, Cr, Fe, and Ni in cm**2/g, given the photon energy in eV. The file TOTLXS.FOR contains a single function that returns the effective cross section in cm**2/H atom, given the photon energy in eV and a set of seventeen relative abundances in log10. If standard abundances (as assumed by Morrison and McCammon) are to be used, the file SIGISM.FOR contains a function implementing the MM polynomials that also returns the effective photoelectric cross section in cm**2/H atom, given the photon energy in eV. It executes much faster than TOTLXS, but gives the same results as TOTLXS called with MM relative abundances. All of these routines are valid only over the photon energy range 30 - 10,000 eV.
CDS 1994 Mar 09 UNKNOWN UNKNOWN * 12 May 1992 --- Release date * 16 Dec 1992 --- Note that He cross sections do not include autoionization levels that increase the cross sections about 15% near 60 eV. A correction will be included soon. There is also some increase in the He cross section at higher energies. * 23 Sep 1993 --- Helium absorption routine updated to version 2.0. This subroutine replaces the previous version of HELIUM which calculated mass absorption coefficients based on Henke's data (Henke, B. L., et al., (1982), Atomic and Nuclear Data Tables, 27, 1). This version of HELIUM returns mass absorption coefficients which are in better agreement with the best experiments as well as theoretical models (see Chen, W. F., Cooper, G., and Brion, C. E., 1991), Phys. Rev. A, 44, 186). This fortran-77 version of the subroutine is based on Pat Jelinsky's program written in C (obtained from EUVE Archive). The new routine now includes the most prominent Fano features near 60 eV. Aside from these auto-ionization feature, the maximum difference in the normal-abundance total cross section is about +20% near 150 eV, with a nearly constant 10% increase from 500 eV to 6 keV. (The cross section for helium alone is increased by more than a factor of three at 5 keV.) The old HELIUM subroutine is now included as file HEL_OLD.FOR. Note that SIGISM.FOR has NOT been updated, and still returns the cross sections of the Morrison & McCammon paper. TOTLXS called with normal abundances will no longer produce the same results. VI_62.xml Orbital, Precessional, and Insolation Quantities for the Earth from -20 Myr to +10 Myr 6063 VI/63 Orbital, Precessional, and Insolation Quan for Earth Orbital, Precessional, and Insolation Quantities for the Earth from -20 Myr to +10 Myr J Laskar F Joutel F Boudin Astron. & Astrophys. 270 522 1993 1993A&A...270..522L Earth Solar system This catalog contains La93 software package which consists of seven FORTRAN codes, some input parameter files (*.par), and nominal orbital, precession, and climatic solution files (*.ASC). They are developed for computing the solution for the precession and obliquity of the Earth for various values of the tidal effect of the Moon (CMAR) and the dynamical ellipticity of the Earth (FGAM). This solution, issued from the orbital solution La90 (Laskar 1990), which is similar to La93(CMAR, FGAM), namely La90=La93(0.,1.), provides the necessary data for the computation of insolation at the surface of the Earth from -20 Myr to +10 Myr. Note when including the tidal dissipation, e.g., La93(1.,1.), this solution presents very good agreement with the 3 Myr numerical integration of Quinn et al. (1991). Additionally, the included routines allow one to test various hypotheses of long term changes in the tidal forces due to the Moon, or in the changes of dynamical ellipticity of the Earth. The files and software of this package can be used in three different manners: 1) Construction and Use of the nominal solution La93(0,1) The ASCII files ORBEL*.ASC contain the nominal orbital solution. The ASCII files PREC0*.ASC contain the nominal precession solution. The ASCII files CLIVAR0*.ASC contain the nominal climatic solution. The files PREC*.ASC and CLIVAR*.ASC can also be generated from the enclosed files. For the computation of insolation quantities, the user will execute the 'prepinsol' step, and then 'insola'. 2) Construction of a parameterized La93(CMAR, FGAM) new solution The user reconstructs a complete La93(CMAR, FGAM) solution. The compilation of all required programs is obtained by running the command 'make' on a Unix machine. The preparation step 'prepa' needs to be done once, in order to prepare the necessary binary files. Then 'integ' will construct the new solutions for the given parameters (CMAR, FGAM) Alternatively, change in the Makefile the values of CMAR and FGAM before running the 'make clean' command (removes the files computed using the preceding values of CMAR and FGAM), and 'make La93'. 3) Changes in the model of precession, for example to take into account some feedback resulting from redistribution of the ice on the Earth resulting from climate changes. In this case, and in this case only, the user needs to edit the FORTRAN file integ.f More precisely, the subroutines which can be eventually modified are SUBROUTINE INIPRE(IPT) SUBROUTINE PRECES(t,AK,AH,AQ,AP,DK,DH,DQ,DP,AKI,DKI) The users may also want to adapt the driver INTEG to his specific needs ***************************************************************************** * * * NOTICE: * * * * This software can be freely copied and distributed provided that: * * * All the included files are kept together. * * * This notice is included in the distribution * * * no changes or alterations are made on the distributed files * * * * Any changes can be performed on the FORTRAN files, for specific use, * * but these changes cannot be included in the distribution files, and * * reference to the original programs should be included. * * * * WARNING: * * This software is not designed to be used in any possible conditions, * * and is not presently in a definite version. * * * * In particular, the user must take care that the starting and ending * * times for which he computes data are contained in the necessary files. * * The stepsize should also be the same. * * * * THE OBJECT OF THIS WORK IS TO PROVIDE A USEFUL TOOL FOR THE PALEOCLIMATE * * COMMUNITY. ANY COMMENTS OR WISH FOR IMPROVEMENTS ARE WELCOME. * * * * Authors: J. Laskar, F. Joutel and some other contributions * * (c) Astronomie et Systemes Dynamiques, Bureau des Longitudes, Paris * * (1993) * * Jacques Laskar * * Astronomie et Systemes Dynamiques, * * Bureau des Longitudes * * 77 av. Denfert-Rochereau * * 75014 Paris * * email: laskar@cosme.polytechnique.fr * * * *****************************************************************************
Normal orbital solution La93(0,1), before present years (-20Myr to 0) Normal orbital solution La93(0,1) after present years (0 to +10Myr) t Time from J2000 in 1000 years 1000yr k k = e * cos (longitude of perihelion) e: eccentricity i: inclination from J2000 ecliptic --- h h = e * sin (longitude of perihelion) --- q q = sin(i/2) cos (longitude of node) --- p p= sin(i/2) sin (longitude of node) --- Nominal solution La93(0,1) before present years (-20Myr to 0) Nominal solution La93(0,1) after present years (0 to +10Myr) t Time from J2000 in 1000 years 1000yr eps obliquity (radians) rad phi general precession in longitude (radians) rad Usual climatic variables in Nominal solution La93(0,1) before present years (-20Myr to 0) Usual climatic variables in Nominal solution La93(0,1) after present years (0 to +10Myr) t Time from J2000 in 1000 years 1000yr e Eccentricity --- eps obliquity (radians) rad CP e*sin(long of perihelion from moving equinox) --- J. Laskar Bureau des Longitudes C.-H. Lyu Hughes STX/NASA 1996 Aug 22 UNKNOWN UNKNOWN Detailed description of the Program -- The program consists of several steps prepa : preparation step. This step generates the necessary binary files from the ASCII files containing the elliptical elements of the Earth every 1000 yr, from -20Myr to +10 Myr from the solution La90. THE USER should edit the file of command prepa.par run prepa two new files : nomfich and nomficder will be created containing the necessary data for the remaining steps for the time span from datedebut to datefin. (a user can choose to work only from -10Myr to 0) integ : integration step. This step is the integration of the equations of precession for various values of the tidal effect, and of the dynamical ellipticity of the Earth. THE USER should edit the file of command integ.par run integ THE USER will be prompted for the values of CMAR and FGAM during the execution of the program climavar : computation of the usual climatic variables prepinsol : preparation of the insolation computations insola : interactive insolation computations ******************************************************************** * NOTE: in prepa.par, integ.par, and prepinsol.par, * * the starting date 'datedebut' and final date 'datefin' * * need to be compatible, otherwise unexpected behaviour will occur.* * In the distributed files, these are set * to -20 Myr and 10 Myr, * * in order to obtain the examples ASCII files of the * * nominal solution. But the user can reduce this to a much shorter * * interval in order to gain computing time and disk space. * ******************************************************************** PREPA This step uses the parameter file prepa.par with the following meaning: nomascpos: ASCII file for positive time (IN) nomascneg: ASCII file for negative time (IN) nomfich : Binary file for elliptical elements (OUT) nomficder: Binary file for derivatives (OUT) datedebut: starting time (Myr) datefin : ending time (Myr) ( -20 <= datedebut < datefin <= +10 ) statut : 'new' or 'unknown' status of the created files Example of prepa.par: -------------------------- &NAMSTD nomfich = 'ELL.BIN', nomfichder = 'DER.BIN', nomascpos = 'ORBELP.ASC', nomascneg = 'ORBELN.ASC', datedebut=-20.D0, datefin=10.D0, statut='unknown' &END -------------------------- The user may restrict himself to e.g. -2Myr to 0 by putting instead datedebut=-2.D0 datefin=0.D0 The output of the 'prepa' command gives the following output: Solution La90-La93 for the Earth La93.prepa version 0.8 preparation step (c) ASD/BdL (1993) ASCII file for positive time : ORBELP.ASC ASCII file for negative time : ORBELN.ASC Binary file for elliptical elements : ELL.BIN Binary file for derivatives of ell. el : DER.BIN starting time (Myr) : -20.00000000000000 ending time (Myr) : 0.0000000000000000E+00 The file ELL.BIN is created. The file DER.BIN is created. The preparation step is completed normally (Duration: about 15 minutes are necessary on a Sparc2 station) INTEG This step uses the parameter file integ.par with the following meaning: nomfich : binary file for the elements t,k,h,q,p this file is computed in the preparation phase prepa. (IN) nomfichder : binary file for the derivatives of the elliptical elements. This file is computed in the preparation phase prepa. (IN) pas : integration step (in years). The default, and advised value is 200 nechant : sampling step. The results are written in the files every nechant*pas years. default nechant = 5 the files gives positions every 5*200 = 1000 years datefin : ending time (Myr) (>=0) datedebut : starting time (Myr) (<=0) ecritpos : 'oui' for output in an ASCII file for positive times 'non' screen output ecritneg : 'oui' for output in an ASCII file for negative times 'non' screen output statut : status of the created files ( 'new' or 'unknown' ) fichrespos : name of ASCII file for positive times t,eps,phi (OUT) t : time (unit = 1000yr) eps : obliquity (radians) phi : general precession in longitude (radians) fichresneg : name of ASCII file for negative times t,eps,phi (OUT) t : time (unit = 1000yr) eps : obliquity (radians) phi : general precession in longitude (radians) Example of integ.par -------------------------- &NAMSTD nomfich = 'ELL.BIN', nomfichder = 'DER.BIN', pas = 200, nechant=5, datefin= 10.D0, datedebut= -20.D0, statut= 'unknown', ecritpos = 'oui', ecritneg = 'oui', fichrespos = 'PRECP.ASC', fichresneg = 'PRECN.ASC' &END -------------------------- The dialog of the 'integ' command gives the following output: La93.integ version 0.8 integration step (c) ASD/BdL (1993) stepsize (yrs) default : 200 : 200.0000000000000 print every 5 step starting time (Myr) : -5.000000000000000 ending time (Myr) : 0.0000000000000000E+00 save results for positive time : oui save results for negative time : oui ASCII file for positive time : PRECP.ASC ASCII file for negative time : PRECN.ASC status of created files : unknown Relative change of dynamical ellipticity ENTER gamma/gamma_0 (default 1) 1 <<<<<<----------------------------------- the user need to answer FGAM = 1.000000000000000 Relative tidal effect 0 : no tidal effect 1 : -4.6 D-18 seconds**-1 ENTER cmar (default 0) 0 <<<<<<----------------------------------- the user need to answer CMAR = 0.0000000000000000E+00 Informations for internal check VITESSE ANGULAIRE DE LA TERRE 474659981.5971373 PRECESSION EN ASCENSION DROITE 5038.783333037391 ELD 3.2800511416867092E-03 RFL0 34.42998531044029 RFL1 -2.6896187697037889E-03 RFL3 3.3459472599329403E-04 RFS 15.97940304351487 RFL0+RFL1+RFL3+RFS 50.40703332991146 CP1,CP2,CP3,CP4 EN SECONDES PAR AN 37.52660322621580 -1.5651731683509029E-03 8.2602928316139284E-05 34.81861759592061 AK1 0.0000000000000000E+00 AK2 0.0000000000000000E+00 (Duration: about 15 minutes are necessary on a Sparc2 station) ************************************************************ * REMARK: when one asks for negative and positive time, * * the user is prompted twice for the preceding questions * ************************************************************ CLIMAVAR After this integration step, if the user prefers the usual climatic variables, he can run the small program climavar which is provided as a FORTRAN source code; the parameters of climavar are taken in climavar.par with similar definitions as in the preceding steps. Alternatively, one can execute make climate INSOLA The two routines prepinsol and insola are designed to compute all necessary insolation quantities derived from the orbital and precessional quantities computed above. They are given on the form of FORTRAN code, so the user can check if they correspond to his needs. He can also design his own insolation routines. A preparation step prepinsol is necessary prior to execution of 'insola'. This preparation step will construct a binary file with the useful quantities. a) set the parameters of prepinsol.par Example: &NAMSTD nomascpos = 'ORBELP.ASC', nomascneg = 'ORBELN.ASC', nomprecpos = 'PRECP.ASC', nomprecneg = 'PRECN.ASC', nomfich = 'SOLCLI.BIN', datedebut = -20.D0, datefin = 10.D0, statut ='unknown' &END b) run prepinsol (these steps are automatically done with the 'make climate' command) For the actual computations of the insolation parameters, the user has to: a) set the parameters of insola.par; in this file, the 'so' parameter refers to the Solar constant expressed in W/m2. Example: &NAMSTD nomfich = 'SOLCLI.BIN', pas = 1.D3, datedebut = -1.D0, datefin =0.D0, statut='unknown', so = 1350.D0, &END b) run insola insola is a self documented program; For more details, the user can refer to La93 (reference above) VI_63.xml Recombination line intensities for hydrogenic ions. IV. Total recombination coefficients and machine-readable tables for Z=1 to 8 6064 VI/64 Recombination line intensities for hydrogenic ions Recombination line intensities for hydrogenic ions. IV. Total recombination coefficients and machine-readable tables for Z=1 to 8 P J Storey D G Hummer Mon. Not. R. Astron. Soc. 272 41 1995 1995MNRAS.272...41S Atomic physics atomic data atomic processes line: formation Line emissivities, effective recombination coefficients, opacity factors, departure coefficients and total recombination coefficients are calculated for hydrogenic ions with Z<=8. There are 162 primary files labelled rZCTTTT.d, where Z=1,2,..,8 is the ionic charge C=a or b is the Case in the sense of Baker and Menzel (1938) (A for a nebula transparent to Lyman line radiation, B for an opaque nebula) TTTT=0.01Te is a reduced temperature variable. There are 9 values of electron densities (log(Ne)=2(1)10) for case A, and 13 (log(Ne)=2(1)14) for case B. The structure of these files is detailed in section 4 of the MNRAS paper. There are 16 secondary files labelled eZC.d, where Z=1,2,..,8 is the ionic charge C=a or b is the Case in the sense of Baker and Menzel (1938) which contain emissivities and total recombination coefficients. These files are accompanied by an interactive data server intrat.f. Please refer to section 5 of the MNRAS paper which details the usage of the program. CGS units are used, meaning that => densities are expressed in cm-3 => emissivities are expressed in erg.s-1.cm-3 (10-7W.cm-3) => effective recombination coefficients are expressed in cm3.s-1
Francois Ochsenbein CDS 1995 Jul 01 Peter J. Storey <pjs@starlink.ucl.ac.uk> VI_64.xml Numerical expressions for precession formulae and mean elements for the Moon and the planets. 6066 VI/66 Precession Formulae and Mean Elements for Moon and Planets Numerical expressions for precession formulae and mean elements for the Moon and the planets. J L Simon P Bretagnon J Chapront M Chapront-Touze G Francou J Laskar Astron. Astrophys. 282 663 1994 1994A&A...282..663S Solar system Ephemerides celestial mechanics, stellar dynamics planets and satellites: general Moon The files given here refer to the paper A&A 282, 663 (1994) which concerns the following topics: - numerical expressions for the precession quantities, - mean elements for Moon and planets, from Mercury to Neptune, - formulae for computing approximate ephemerides for Moon and planets. The files concern only precession and approximate ephemerides of the planets. The numerical expressions of precession are yielded by files : prctable.doc, prcbdl94.f, prcupdt.f. The formulae for computing approximate ephemerides of the planets are available in file : planetap.f. There is no file for the mean elements of Moon and planets because these quantities are of a more specific use. Approximate lunar ephemerides may be computed from tables in: Chapront-Touze M., Chapront J. (1991) "Lunar Tables and Programs from 4000 B.C. to A.D. 8000" Willmann-Bell, Inc., Richmond, Virginia, USA.
prctable.doc Table of precession quantities BDL94. BDL 1994 May 12 Authors' Address: Bureau des Longitudes, URA 707. 77, Avenue Denfert-Rochereau 75014, Paris, France. VI_66.xml Bibliographic Catalogue of Variable Stars (BCVS), Part 1 6067 VI/67 Bibliographic Cat of Variable Stars Bibliographic Catalogue of Variable Stars (BCVS), Part 1 H Huth W Wenzel CDS Bull. 20 105 1981 1981BICDS VI/68 : BCVS Part II 1994 Update Bibliography Stars, variable This catalog of variable star data is an update of the contents of the "Geschichte und Literatur des Lichtwechsels der Veraenderlichen Sterne" which was complete only up to 1958. It is based on a card catalog maintained at the Sonneberg Observatory. In general, each entry contains the name of the variable and the authors name and reference for the published information. The Bibliographic Catalogue of Variable Stars was described in detail by W. Wenzel in Bull. Inf. CDS 20, 105; the present edition incorporates reformatted data from the original catalogue (catalogue VI/35) and the first Supplement (catalogue VI/38). Many corrections have been performed, and references up to 1987 have been added.
Catalog Data Const Constellation Name --- Name Name in constellation --- Code Coded name of star The coded name is made of: -2 digits for Constellation (values 01 to 88) -1 digit indicates a "common" variable name (value 0), a greek letter (value 1) or a latin letter (value 2) -4 digits designate the variable letter(s) or number, as 0001=R ... 0009=Z, 0010=RR, ... 0018=RZ, ... 0055=AA ,,, 0334=QZ, 0335=V335 ... --- Year Year of publication yr Ref Text of reference '*' separates authors, journal, volume, and page number --- modified by James E. Gass SSDOO/ADC 1998 Oct 27 VI_67.xml Bibliographic Catalogue of Variable Stars (BCVS), Part II Update 1994 6068 VI/68 Bibliograpy of Variable Stars Bibliographic Catalogue of Variable Stars (BCVS), Part II Update 1994 S Roessiger H -J Braeuer Bull. Inf. CDS ??? ??? in press BICDS VI/67 : Bibliographic Catalogue of Variable Stars (BCVS) Part 1 Bibliography Stars, variable This catalogue is a supplement of the Bibliographic Catalogue of Variable Stars (BCVS), which was described by W. Wenzel in Information Bulletin of the CDS, no.20, p.105 (1981). It comprises the bibliography of the named variable stars at our disposal that have been published from 1982 up to the beginning of 1994 (as far as this has been possible). A diminutive part of the data refers to the time prior to 1982 concerning literature which had not been at our disposal before closing the main part of the BCVS. The present file also includes the references for all variable stars that have been newly named since 1982 (name-lists no. 67, 68, 69, 70, 71 of the IAU) with references collected in Sonneberg (possibly from literature published before 1982). The shape of the entries differs slightly from that in the main part of the BCVS. The innovation consists in the addition of keywords giving a concise characterization of the contents of the individual publication. The application of keywords has been traditional practice at Sonneberg Observatory and is particularly adapted to observation and study on variable stars in the optical range. The entries have the following structure: - name of the variable star - year of publication - name of author(s) - name of publication (mostly abbreviated) - volume (or fascicule) and page numbers - keyword(s) (not in all entries) The abbreviations used for the names of the publications are listed in the file "abbr.lis"
The Catalogue Const Constellation Name --- Name in constellation --- Year of publication yr Sep Indicator of several years (/) or doubtful year (?) --- Ref Text of reference and keywords. The carret (^) separates the authors and journal from keyword parts; each keyword consists in a single character which explanation is found in file "keys" --- Francois Ochsenbein CDS 1994 Jun 13 VI_68.xml Atomic spectral line list 6069 VI/69 Atomic Spectral Line List Atomic spectral line list R Hirata T Horaguchi Department of Astronomy, Faculty of Science, Kyoto University, and National Science Museum, 3-23-1 Hyakunin-cho, Shinjuku-ku, Tokyo ??? ??? 1995 1995 Atomic physics Multiplet Spectroscopy This compilation is aimed at providing a general catalog of atomic lines for comparatively low-ionized species, laying emphasis on their transition probabilities, and consists of three files: file 1: Description and status report for each ion(this file), file 2: Table of references(1,144 references from Kelly(1987,=K003), and 655 additional references) file 3: Atomic line table The catalog.dat file includes wavelength, line classification, laboratory intensities and transition probabilities. We treat mainly permitted lines. Damping constants and collision cross section are out of scope. We make an effort to be as self-consistent as possible, for examples, between wavelength and energy levels, and in the multiplet-number designation. The former example enables us to find misprints in literatures. The latter example requires that we frequently change the multiplet members or to re-define the multiplet number itself, when energy level or term designation are altered from those of Moore. Predicted wavelengths are calculated by the dispersion formula given by B.Edlen(1966,Metrologia, 2, p71), except for platinum lines where main source(Reader et al. 1988,=R023) employed Peck & Reeder's(1972,J. Opt.Soc.Americ. 62, p158) three-term formula. Based on this compilation, the data retrieval system ATMLINE is open to Japanese users through Data Processing Center of Kyoto University, since 1989. Main features of our list are as follows: *wavelength region : 1.4 to 10,000nm *elements : z=1 to 92(with some heavy ions missing) *ionization stage : all for z<=8, I to VI for z=9-30, I to II or V for z=31-92 *total number of lines : 629,771 lines. The main sources are as follows: 1. Starting files are Kurucz(1975,1989,=K000, K002) which give semi-empirical gf-values for many ions. 2. Energy levels are adopted from recent compilations(e.g., Sugar & Corliss(1985,=S001) or individual works. 3. We merged Kelly's(1983,=K001) list into our file(wv<3500A). We make an effort to collect the best wavelength values, especially for the region above 3500A. Thus, this compilation can be regarded as an extension of Kelly's ultraviolet line table towards optical and infrared regions, though still incomplete. 4. The gf-values are first taken from the several compilations( e.g.,Martin et al.(1988,=M005), Fuhr et al.(1988,=F005), Wiese & Martin(1980,=W002), Wiese et al.(1966,1969,=W001) and Morton (1991,=M013)). We also adopted published results of Opacity Project(see Seaton,M.J. 1987, J.Phys. B20, 6363), and the other recent articles(about 360 references). 5. The multiplet numbers are from Moore's Multiplet Tables(refs. 0488 & 1015). We adopt Moore's new compilations for C,N,O, and Si(refs.0504,0507,0510,0511,0521,0522,0523,0628,M012, and M058). Adelman's compilation for Mn I and Co II are also adopted. 6. Laboratory intensities are taken from various sources, though incomplete at present. The most important source is Meggers et al.(1975,=M003). Kelly's(1983,=K001) intensities are kept in priciple(wv<3500A).
The catalogue of Atomic Spectral Lines ION Ion number (e.g. 2602=Fe II) --- lambda Wavelength in Angstrom 0.1nm n_lambda Note on lambda: number=1 These are given only for 1999.3520A <= lambda < 2000.0000A. Vacuum wavelength below 1999.3520A, air wavelength above 2000.0000A. - = vacuum wavelength + = air wavelength --- Hyb Hybridation number=2 These are introduced, for example, for the mean wavelength of the multiplet. numerals = number of component # = composite line - = component for which composite wavelength is given elsewhere --- r_lambda Reference number for lambda --- Rem1 Remark number=3 This terminology was introduced by Kelly(1983,=K001). 'F' : forbidden 'R' : forbidden,quadrupole 'S' : standard wavelength 'M','W': secondary standard 'h' : hyperfine structure detected or hyperfine component 'i' : isotope --- Rem2 Remark number=4 This terminology was introduced by Kelly(1983,=K001). 'S' : solar 'F' : flare 'h' : hyperfine structure detected or hyperfine component 'i' : isotope --- Rem3 Remark number=5 This terminology was introduced by Kelly(1983,=K001). 'A' : upper state autoionizing 'N' : unclassified '?' : line appeared in K000 or K002, but is rejected from current term analysis. --- Rem4 Remark number=6 This terminology was introduced by Kelly(1983,=K001). 'A' : observed in absorption 'M' : unclassified, uncertain ionization 'N' : unclassified 'P' : predicted 'Q' : questionable or uncertain classification '?' : same as in Rem3 --- gf1 Primary log gf value --- q_gf1 quality of gf1 number=7 The accuracies in the NBS compilations(ref.W001,W002,W003, Y001,F001,F002) are converted into 'symbolic' numerical values (dex) as follows: '003'(AA+) '004'(AA) '005'(AA-) '012'( A+) '013'( A) '014'( A-) '03 '( B+) '04 '( B) '05 '( B-) '09 '( C+) '10 '( C) '11 '( C-) '17 '( D+) '18 '( D) '19 '( D-). A question mark is introduced for the line in K002 whose energy level value differs considerably from the current term analysis. We re-calculated the wavelength, following the recent interpretation, but the gf-value is kept unchanged. Note that this mark is not introduced for K000. If lambda differs from lamKP greatly, the gf value in K000 is also questionable. numerals: 1,000 x error(dex) ' E' : error>50% '? ' or ' ?': questionable ' <' : upper limit ' L' : our conversion from multiplet gf into its components (LS coupling) ' EL' : combination of 'E' & 'L' above --- r_gf1 Reference number for gf1 --- gf2 Secondary log gf value --- q_gf2 Quality of gf2, the meaning is same as in q_gf1 --- r_gf2 Reference number for gf2 --- Int1 Laboratory intensity 1 number=8 The last column is usually used for the quality: a asymmetric b blend, double c complex d diffuse, broad h hazy l shaded towards longer wavelength m masked n nebulous p perturbed by close line r reversed s shaded towards shorter wavelength w wide + slightly larger than - slightly less than > greater than ? questionable : uncertain All six columns may be occupied by the intensity value itself in the case of wide range intensity scale. --- r_Int1 Reference number for Int1 --- Int2 Laboratory intensity 2 number=8 The last column is usually used for the quality: a asymmetric b blend, double c complex d diffuse, broad h hazy l shaded towards longer wavelength m masked n nebulous p perturbed by close line r reversed s shaded towards shorter wavelength w wide + slightly larger than - slightly less than > greater than ? questionable : uncertain All six columns may be occupied by the intensity value itself in the case of wide range intensity scale. --- r_Int2 Reference number for Int2 --- r_class Reference number for line classification --- Mult Multiplet number number=9 The first column is usually 'U'(Moore's ultraviolet multiplet tables=ref.0488) or 'V'(ref.1015). See section C for others. --- r_Mult source of multiplet number number=10 'M' : Moore(refs.0488 or 1015) '=' : doubly defined in refs.0488 & 1015 'A' : Moore's new multiplet tables(C,N,O,Si) or Adelman's table(Mn I & Co II) 'K' : Kelly(1983,=K001) 'N' : NBS gf-compilation(W001 etc.) 'Q' : our finding or our re-definition other symbols: see section C of document for individual ion --- E1 Lower energy level (cm^(-1)) cm-1 n_E1 Note on E1: number=11 alphabetic: unknown constant to be added to E1 '?' : questionable E1 --- g1 Statistical weight, lower energy level --- n_g1 Remark on g1 number=12 numerals: number of levels concerned '#' : "multiplet" g-value '?' : questionable --- n_E1GA Remark on E1 number=13 'G' : ground level 'A' : level above the first ionization limit --- Term1 Lower term number=14 We usually adopt Kelly's(1983,=K001) expression for the term designations other than the LS coupling. --- r_E1 Reference number for E1 --- E2 Upper energy level (cm^(-1)) --- n_E2 (15) --- g2 statistical wt of upper energy level --- n_g2 remark on g2, same as in n_g1 --- n_E2GA remark on E2, same as in n_E1GA --- Term2 Upper term number=14 We usually adopt Kelly's(1983,=K001) expression for the term designations other than the LS coupling. --- r_E2 reference number for E2 --- gfKP log gf given by Kurucz(K000 or K002) --- lamKP original wavelength in K000 or K002 0.1nm The references Refno Reference number numeric code: defined by Kelly(1987,=K003) alphanumeric code: our definition --- Year Published year yr Text free format: from 11- : authors after * : journal after % : contents after # : number of lines appearing in the paper --- explain.txt Description and Explanations Ryuko Hirata NAOJ 1994 Dec 21 VI_69.xml A revised version of the Identification List of Lines in Stellar Spectra (ILLSS) Catalogue 6071 VI/71 Revised version of the ILLSS Catalogue A revised version of the Identification List of Lines in Stellar Spectra (ILLSS) Catalogue R Coluzzi Bull. Inf. CDS 43 7 1993 1993BICDS..43....7C VI/84 : UVILLSS Catalogue (Coluzzi 1996) Moore, C.E.: 1972, "A Multiplet Table of Astrophysical Interest, Revised Edition", Nat. Stand. Ref. Data Ser., Nat. Bur. Stand, 40. Seitter, W.C.: 1969, "Atlas for Objective Prism Spectra", Ferd. Dummlers Verlag. Bonn 1970 Atomic physics Spectroscopy This catalogue is a revised version of the Identification List of Lines in Stellar Spectra and now lists wavelength, spectrum, multiplet number, intensity, ionisation potential and stellar type reference for lines in the region 2951 to 13164 Angstroems. (This catalogue was announced as number III/171)
The ILLSS Catalogue, organized as a table lambda Wavelength in Angstroems 0.1nm Element Element (or molecule) name and spectrum --- Z Atomic element number, zero if not applicable --- Ion Electronic charge --- n_lambda Note concerning the line number=1 The notation is the following: ' ' for observed line '*' for blend 'P' for predicted line 'F' for forbidden predicted line 'f' for forbidden line observed in the laboratory 'N' for nebular forbidden measured line 'L' for laboratory forbidden measured line 'A' for auroral forbidden measured line 'C' for coronal forbidden measured line '?' for which the element attribution is uncertain --- Multiplet Multiplet number --- RefL Reference of intensity number=2 the reference is relative to the Element ; the following notations are used: - A colon : indicates that the intensity is not the first or second choice. - The letters have the following meaning: 'd' double 'g' ghost 'l' shaded to longer wave-length 'n' diffuse or hazy 'N' very diffuse or very hazy 'p' part of band 'r' narrow self-reversal 'R' wide self-reversal 's' shaded to shorter wave-length 'tr' trace 'w' wide(fine structure type),broad or complex 'W' very wide(fine structure type) or very broad However, the intensity is marked as '[????]' for the 2 records present in part II (Finding List) and not in part I (Table of Multiplets) of Moore catalogue: 10752.99 FeI (1352) and 10849.68 FeI (1352) --- Intens Intensity with Moore notation number=2 the reference is relative to the Element ; the following notations are used: - A colon : indicates that the intensity is not the first or second choice. - The letters have the following meaning: 'd' double 'g' ghost 'l' shaded to longer wave-length 'n' diffuse or hazy 'N' very diffuse or very hazy 'p' part of band 'r' narrow self-reversal 'R' wide self-reversal 's' shaded to shorter wave-length 'tr' trace 'w' wide(fine structure type),broad or complex 'W' very wide(fine structure type) or very broad However, the intensity is marked as '[????]' for the 2 records present in part II (Finding List) and not in part I (Table of Multiplets) of Moore catalogue: 10752.99 FeI (1352) and 10849.68 FeI (1352) --- n_Intens Notes about the Intensity number=2 the reference is relative to the Element ; the following notations are used: - A colon : indicates that the intensity is not the first or second choice. - The letters have the following meaning: 'd' double 'g' ghost 'l' shaded to longer wave-length 'n' diffuse or hazy 'N' very diffuse or very hazy 'p' part of band 'r' narrow self-reversal 'R' wide self-reversal 's' shaded to shorter wave-length 'tr' trace 'w' wide(fine structure type),broad or complex 'W' very wide(fine structure type) or very broad However, the intensity is marked as '[????]' for the 2 records present in part II (Finding List) and not in part I (Table of Multiplets) of Moore catalogue: 10752.99 FeI (1352) and 10849.68 FeI (1352) --- IP Ionisation Potential eV SpTypes List of concerned spectral types --- Regina Coluzzi Oss. Roma Francois Ochsenbein CDS 1997 Mar 27 UNKNOWN UNKNOWN * 31-Aug-1994: file prepared by Regina Coluzzi [Oss. Roma] * 04-Apr-1996: the table illss.dat was created from illss.cat at CDS (F. Ochsenbein) to allow its usage by a database. * 27-Mar-1997: transformed intensities into numeric column and remarks. at CDS (F. Ochsenbein) VI_71.xml Atomic Transition Probabilities, Scandium through Manganese 6072 VI/72 Atomic Transition Probabilities, Sc-Ni Atomic Transition Probabilities, Scandium through Manganese J R Fuhr G A Martin W L Wiese J. Phys. Chem. Ref. Data, Vol. 17, Suppl. 3 ??? ??? 1988 1988atps.book.....F Atomic Transition Probabilities, Scandium through Manganese J R Fuhr G A Martin W L Wiese J. Phys. Chem. Ref. Data, Vol. 17, Suppl. 4 ??? ??? 1988 1988atpi.book.....F Atomic physics NIST, atomic transition probabilities Atomic transition probabilities for Scandium (Z = 21) through Ni (Z = 28) for about 18,300 spectral lines are critically compiled, based on all available literature sources. The transition probability data, oscillator strengths, and line shape data were collected, catalogued and evaluated by the Data Center on Atomic Transition Probabilities at the National Institute of Standards and Technology, USA (NIST).
Transition probabilities At_sym Element --- Spect_No Stage of Ionization --- Allowed Transition type - Allowed or Forbidden --- ATP_mult Multiplet Number --- Seq_No Sequence number within Multiplet 0 refers to weighted averages of line values. --- Lo_conf Lower energy level configuration --- Up_conf Upper energy level configuration --- Lo_term Lower energy level term --- Up_term Upper energy level term --- Mult_No Multiplet Table Number The Multiplet Table Number Refers to Multiplet Tables by Charlotte Moore. --- Pre_Wave Wavelength Prefix A square bracket "[" indicates approximate calculated or extrapolated values --- Wave Wavelength 0.1nm ELo Lower Energy Level cm-1 EUp Upper Energy Level cm-1 Gi g(i) statistical weight lower level --- Gk g(k) statistical weight upper level --- Aki A(k,i)transition probability (in 10^8 s-1) 0.1GHz fik f(i,k) oscillator strength --- S line strength (atomic units) The line strength is given in atomic units. A cross reference table for converting between S, f(i,k), A(i,k) is given in the source reference. Some authors have used a definition of the line strength for E2 transitions which yields a 50% higher value than employed here and in earlier NBS transition-probability compilations. --- log(gf) log gf --- Type Forbidden transition type Type indicates the forbidden transition types. E1 = electric dipole transition E2 = electric quadrupole transition M1 = magnetic dipole transition M2 = magnetic quadrupole transition --- Acc accuracy rating - uncertainties The ratings for the uncertainties are: A = within 3% B = within 10% C = within 25% D = within 50% E = greater than 50% +,- = often a further distinction in the uncertainty labels was made by assigning a plus or minus to indicate the lines are estimated to be somewhat better or worse than similar lines. c, 1, 2 = undefined --- NIST_ref NIST Data Center literature reference code Abbreviations appearing are: ls : LS coupling rules applied n : normalized to a scale different from that of the author interp.: derived by an interpolation technique rather than taken directly from the literature The NIST reference source code list is not available in electronic form as part of this data set. --- N.P.M. Kuin NSSDC/ADC 1994 Nov 09 UNKNOWN UNKNOWN The following errors were found and corrected after checking the printed version: (1) in record 7967 an underscore in the exponent was replaced by a minus sign; (2) a comma in the A(k,i) field number was replaced by a dot; (3) the S field in records 9840 and 14850 was replaced by the printed value; (4) the bar sign in record 211 was found to be spurious. In addition to these changes, the opening and closing brackets around the exponent in the Aki, fik, and S fields were replaced by the "E" for the exponent followed by the exponent value. The notes "a" following the closing bracket were found to be unnecessary and removed. The format for the Aki, fik and S fields could not be specified as an F format, nor could the values be aligned since many values were found to be integer, but all non-numeric characters have now been removed from those fields. VI_72.xml Selected Tables of Atomic Spectra (O II) 6073 VI/73 Atomic Spectral Lines Data OII, Mg, Al, S, Sc Selected Tables of Atomic Spectra (O II) W C Martin V Kaufman J. Phys. Chem. Ref. Data, in preparation ??? ??? 1992 1992 Selected Tables of Atomic Spectra (O II) V Kaufman W C Martin J. Phys. Chem. Ref. Data, Vol. 20 83 1991 1991 Selected Tables of Atomic Spectra (O II) V Kaufman W C Martin J. Phys. Chem. Ref. Data, Vol. 20, No. 5, p. 775 ??? ??? 1991 1991 Selected Tables of Atomic Spectra (O II) W C Martin R Zalubas A Musgrove J. Phys. Chem. Ref. Data, Vol. 19 821 1990 1990 Selected Tables of Atomic Spectra (O II) V Kaufman J Sugar J. Phys. Chem. Ref. Data, Vol. 17 1679 1988 1988 Atomic physics NIST, Atomic Spectral Line Data Atomic Spectral Lines Data O II, Mg I-XII, Al I-XIII, S I-XVI, Sc I-XXI. Using recent critical compilations of atomic energy levels, the authors calculate wavelengths (or wave numbers) from the differences of the energy levels. Results are given along with the observed values for all classified lines. Unless otherwise noted, the calculated values are in general more accurate than the observed values wherever the two values differ significantly. Some observed lines are classified as unresolved blends of two or more transitions. The calculated wavelength for each of the main components of such a blend is listed, or in some cases the calculated wavelength of the probable strongest component.
spectral line data for OII, MgI-XII, AlI-XIII, At_sym Atomic element Atomic symbol of atomic element --- Spect_No Stage of Ionization Stage of ionization or spectrum number. The spectrum numbers are "1" for Roman I (neutral atom), etc. --- Mult_No Multiplet Number The Multiplet Table Number Refers to Multiplet Tables by Charlotte Moore (i.e., UV10). --- Intens Relative Intensity Relative Intensity (i.e, 1500g,a). The numbers are usually visual estimates related in some way to plate blackening. Some authors limit these estimates to a small range (e.g., 1 to 10) while others reach into the 100,000's. Such numbers are useful within a small wavelength range and are meaningful only for comparing lines of a particular spectrum taken from a particular reference. More meaningful relative intensities obtained with photoelectric or solid-state detectors are given by some authors, especially in the infrared region. In some cases the originally published intensities have been adjusted in particular regions to reduce apparent discrepancies between different observers, etc. Kelly (1987) adjusted the various intensity scales of the original observers to a normalized scale having a maximum intensity of 1000. For some spectra, Kelly's adjusted intensities have been given for some or all of the lines below 2000 A. The following symbols further characterize the lines: M1,M2,E2, ... : magnetic-dipole, magnetic-quadrupole, electric- quadrupole, ... transition bl: blended with another line that may affect the wavelength and intensity. m : masked by another line (no wavelength measurement) d : diffuse, wide, hazy, etc. g : transition involving a level of the ground term. a : observed in absorption. w : ? : --- Code Typesetting Code Typesetting Code. The braces are used for denoting multiply-classified lines or other groupings: { = suppress observed value, intensity and reference } = suppress lower and upper levels and designations C = used when there are only calculated values, and signals suppression of the observed line values. --- Obs_Wave Observed Wavelength Observed Wavelength. Wavelengths in vacuum are given for values below 2000 Angstroms, wavelengths in air for the region 2000-10,000 Angstroms. In the infrared region longer than 10,000 Angstroms vacuum wave numbers are used (instead of wavelengths in air). Wavelengths are in increasing order, vacuum wave numbers in decreasing order. ? : a question mark following the calculated wavelength indicates that the energy level classification of the line is questionable 0.1nm CalcWave Calculated Wavelength 0.1nm Obs_WNum Observed Wave Number cm-1 CalcWNum Calculated Wave Number cm-1 Pre_ELo Lower Level Prefix --- ELo Lower Energy Level cm-1 Suf_ELo Lower Level Suffix +, x, X : uncertainty ] : calculated value ? : A question mark following the upper level indicates the classification is tentative. --- Pre_EUp Upper Level Prefix --- EUp Upper Energy Level cm-1 Suf_EUp Upper Level Suffix --- Lo_conf Lower Level Configuration --- Up_conf Upper Level Configuration --- Lo_term Lower Level Term --- Up_term Upper Level Term --- Lo_J Lower Level J value --- Up_J Upper Level J value --- NIST_ref Reference References for observed wavelengths (i.e, r1,s1), see the published paper. --- P.M. Kuin ADC/NSSDC 1994 Nov 09 UNKNOWN UNKNOWN There are twenty-two fields for each spectral line. Each text field is in columnar format and is left-justified. The numeric fields (F format) are right justified. The fields for wavelength, wave and energy level from the original data file were aligned on the dot. Excessive blanks were removed. VI_73.xml Selected Tables of Atomic Spectra (O II) 6074 VI/74 Atomic Energy Level Data Selected Tables of Atomic Spectra (O II) W C Martin V Kaufman J. Phys. Chem. Ref. Data, in preparation ??? ??? 1992 1992 Selected Tables of Atomic Spectra (O II) W C Martin R Zalubas J. Phys. Chem. Ref. Data, Vol. 10 195 1981 1981 Selected Tables of Atomic Spectra (O II) W C Martin R Zalubas J. Phys. Chem. Ref. Data, Vol. 9 1 1980 1980 Selected Tables of Atomic Spectra (O II) W C Martin R Zalubas J. Phys. Chem. Ref. Data, Vol. 8 817 1979 1979 Selected Tables of Atomic Spectra (O II) W C Martin R Zalubas J. Phys. Chem. Ref. Data, Vol. 12 323 1983 1983 Selected Tables of Atomic Spectra (O II) W C Martin R Zalubas A Musgrove J. Phys. Chem. Ref. Data, Vol. 14 751 1985 1985 Selected Tables of Atomic Spectra (O II) W C Martin R Zalubas A Musgrove J. Phys. Chem. Ref. Data, Vol. 19 821 1990 1990 Selected Tables of Atomic Spectra (O II) J Sugar Ch H Corliss J. Phys. Chem. Ref. Data, Vol. 14, Suppl. No. 2 ??? ??? 1985 1985 Selected Tables of Atomic Spectra (O II) J Sugar A Musgrove J. Phys. Chem. Ref. Data, Vol. 19 527 1990 1990 Selected Tables of Atomic Spectra (O II) J Sugar A Musgrove J. Phys. Chem. Ref. Data, Vol. 20 859 1991 1991 Selected Tables of Atomic Spectra (O II) J Sugar A Musgrove J. Phys. Chem. Ref. Data, Vol. 17 155 1988 1988 Selected Tables of Atomic Spectra (O II) W C Martin R Zalubas L Hagan Natl. Stand. Ref. Data Ser., Natl. Bur. Stand. 60 ??? ??? 1978 1978 Atomic physics NIST, Atomic Energy Level Data This data set is a critical compilation of data on atomic energy levels for atoms and ions. For a number of the ions the levels have been derived or recalculated. In addition to the level value in cm-1 and the parity, the J value and the configuration and term assignments are listed if known. Leading percentages from the calculated eigenvectors are tabulated wherever available.
Atomic Energy Level Data At_Sym Atomic element symbol --- Spect_No Stage of Ionization Stage of ionization or spectrum number. The spectrum numbers are "1" for Roman I (neutral atom), etc. --- Mconf Main Configuration --- Mterm Main Term --- J j value --- P Parity '@' = odd (italics in the publication) blank = even --- Pre_E Level Prefix "[" = calculated value --- E Energy Level cm-1 Suf_E Level Suffix "]" = calculated value "?" = questionable "*" = questionable "+x"= uncertainty --- Pre_g prefix to Lande g factor See the printed documentation for details --- g Lande g factor --- Suf_g suffix to Lande g factor --- Perc1 first leading percentage (eigenvector) --- Conf1 Configuration 1 --- Term1 Term 1 --- Perc2 second leading percentage --- Conf2 Configuration 2 --- Term 2 Term 2 --- Code Percentage Code Percentage code (used to identify "Limit" records and "series" records and to typeset leading percentages) N=print the first percent Q=print percent1, percent2,configuration2, term2 T=print everything --- N.P.M. Kuin ADC/NSSDC 1994 Nov 09 UNKNOWN UNKNOWN There are seventeen fields for each level record. Each field with character values is left-justified. Excessive blanks between the fields were removed. The fields with numeric values were right justified and prefix and suffix were removed to separate columns. The formats for these fields were changed accordingly. VI_74.xml A Simulation Atlas of Tidal Features in Galaxies 6076 VI/76 Simulation Atlas of Tidal Features in Galaxies A Simulation Atlas of Tidal Features in Galaxies S Howard W C Keel G G Byrd J Burkey Astrophys. J. 417 502 1993 1993ApJ...417..502H Morphology Galaxies, peculiar The simulation survey of tidally perturbed galaxies provides images of 84 different encounters that vary orbit tilt of companion orbit, perigalacticon distance ratio of primary galaxy mass to companion mass, and the amount of inert matter in the primary galaxy. In total 1764 galaxy images are available in the survey. This data set contains 84 separate simulations, each simulation is run for 1000 time steps, producing image output of the star particles and gas particles separately every 50 time steps. The first 21 images represent the "gas", and the second 21 images represent the "stars". Time steps for matching "gas" and "stars" are the same. There are [256,256] grid points on a Cartesian coordinate system. The renormalized densities are stored as 8-bit floating point numbers. The data have been put into FITS. Each header specifies the parameters for that simulation. The data compress very well. 97+% compression ratios have been achieved. It is therefore recommended to retrieve the data in compressed form over the network. The individual survey files have been archived in a (UNIX) TAR container called "survey.tar". The survey files have been compressed (*.z extension) using the GZIP compress utility. The size of the TAR container is about 32 Mbytes.
The simulation atlas provides an image dictionary of simulations that span several encounter parameters with fine morphological resolution and includes the effects of self-gravitation. Observers and theorists can then search the dictionary for the parameters that best match a particular observed morphology. The survey uses a self-gravitating, 180,000 particle, two-component ("stars" and "gas") disk with an inert halo. The companion follows a fully 3D self-gravitating orbit. The disk is constrained to two dimensions. The "star" data and the "gas" data are stored as separate images. The n-body code has a polar-coordinate grid especially well suited to simulate disk galaxies. The grid is exponentially spaced in the radial direction and provides increasing resolution from edge to center. Each bin has a constant angular size as seen from the origin. There are 24 radial and 36 azimutal bins which give an effective resolution that matches a 720x720 Cartesian grid. The code combines the speed of a particle mesh code with tree aspects for fine tuned handling of the companion orbit. The code is stable against intrinsic small perturbations. The initial potential for the disk is a finite Mestel (1963) disk which produces a flat rotation curve. The halo is represented by an inert potential set to match the value of the Mestel potential in the disk. The contribution of this potential is either equal to the potential of one disk mass or ten times the potential of one disk mass. Of the 180,00 particles, 126,000 of the are "stars", each having a velocity dispersion in the disk plane that ensures stability against axisymmetric perturbations. The remaining 54,000 "gas" particles have an initial velocity dispersion of 0.0. The particles are not allowed to collide. The initial velocity of the companion is set to match a zero energy orbit. The initial position is far enough away to assure a clean passage. The companion is treated as a point mass. Each simulation runs for 1000 time steps. With 50 steps per crossing time (one crossing time is the time a particle takes to travel a distance of one disk radius traveling at the initial circular orbital speed), there are 314 time steps for one galactic rotation. Assuming a typical disk radius of 20kpc, and a disk orbital speed of 200 km/s, one time step corresponds to about 1.5 million years. Content of the Atlas: The original Atlas contains 86 separate simulations. The 2 simulations with no companion present that were used for testing the stability of the code are absent in this distribution. Each simulation is run for 1000 time steps, producing image output (an image of the star particles and an image of the gas particles) every 50 time steps. The code stores the gas particles and the star particles separately. This data set does not combine them. Therefore, each simulation contains 21 "gas" images and 21 "star" images. The time steps for matching "gas" and "star" images are the same. Each image is stored as a floating point array [256,256]. Each cel contains a scaled floating point number that represents the number of particles in that cell. The data are written as FITS files. The scaling algorithm was chosen to maximize contrast for image display units. The cell containing the companion is set to 35,000 always. Where the zero count is zero, the cell contains the number 0.0. Where the count is non-zero, the cell contains a value of Value = N*64,000/(max cell count for that image) + 2048, where N is the particle count for that cell. The files are listed in the File Summary above. The file name includes the letters "str" or "gas" as appropriate and the letter i followed by the inclination of the companion orbit (in degrees) followed by a running letter. When the letter "r" follows that letter, the rotation is a retrograde orbit. When there is no letter "r" the simulation follows a prograde passage of the companion. The parameter ranges are: - the companion orbit has inclinations of 0, 30, 60, 89 deg. - ratio of halo mass to disk mass (dark matter test) = 1 and 10 - distance of closest approach of companion = 1 and 2 (in terms of galaxy disk radius Ren/Rg - 1=grazing encounter, 2=distant encounter) - ratio of companion mass to primary mass = 0.1, 0.5, 1.0 For each file the parameter ranges are listed in the File Summary table.
str_i0a.fit incl=0 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 gas_i0a.fit incl=0 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 str_i0ar.fit incl=0 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 gas_i0ar.fit incl=0 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 str_i0b.fit incl=0 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 gas_i0b.fit incl=0 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 str_i0br.fit incl=0 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 gas_i0br.fit incl=0 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 str_i0c.fit incl=0 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 gas_i0c.fit incl=0 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 str_i0cr.fit incl=0 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 gas_i0cr.fit incl=0 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 str_i0d.fit incl=0 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 gas_i0d.fit incl=0 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 str_i0dr.fit incl=0 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 gas_i0dr.fit incl=0 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 str_i0e.fit incl=0 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 gas_i0e.fit incl=0 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 str_i0er.fit incl=0 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 gas_i0er.fit incl=0 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 str_i0f.fit incl=0 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 gas_i0f.fit incl=0 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 str_i0fr.fit incl=0 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 gas_i0fr.fit incl=0 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 str_i0g.fit incl=0 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 gas_i0g.fit incl=0 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 str_i0gr.fit incl=0 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 gas_i0gr.fit incl=0 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 str_i0h.fit incl=0 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 gas_i0h.fit incl=0 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 str_i0hr.fit incl=0 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 gas_i0hr.fit incl=0 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 str_i0i.fit incl=0 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 gas_i0i.fit incl=0 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 str_i0ir.fit incl=0 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 gas_i0ir.fit incl=0 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 str_i0j.fit incl=0 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 gas_i0j.fit incl=0 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 str_i0jr.fit incl=0 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 gas_i0jr.fit incl=0 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 str_i0k.fit incl=0 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 gas_i0k.fit incl=0 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 str_i0kr.fit incl=0 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 gas_i0kr.fit incl=0 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 str_i0l.fit incl=0 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 gas_i0l.fit incl=0 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 str_i0lr.fit incl=0 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 gas_i0lr.fit incl=0 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 str_i30a.fit incl=30 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 gas_i30a.fit incl=30 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 str_i30ar.fit incl=30 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 gas_i30ar.fit incl=30 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 str_i30b.fit incl=30 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 gas_i30b.fit incl=30 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 str_i30br.fit incl=30 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 gas_i30br.fit incl=30 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 str_i30c.fit incl=30 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 gas_i30c.fit incl=30 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 str_i30cr.fit incl=30 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 gas_i30cr.fit incl=30 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 str_i30d.fit incl=30 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 gas_i30d.fit incl=30 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 str_i30dr.fit incl=30 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 gas_i30dr.fit incl=30 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 str_i30e.fit incl=30 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 gas_i30e.fit incl=30 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 str_i30er.fit incl=30 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 gas_i30er.fit incl=30 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 str_i30f.fit incl=30 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 gas_i30f.fit incl=30 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 str_i30fr.fit incl=30 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 gas_i30fr.fit incl=30 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 str_i30g.fit incl=30 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 gas_i30g.fit incl=30 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 str_i30gr.fit incl=30 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 gas_i30gr.fit incl=30 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 str_i30h.fit incl=30 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 gas_i30h.fit incl=30 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 str_i30hr.fit incl=30 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 gas_i30hr.fit incl=30 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 str_i30i.fit incl=30 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 gas_i30i.fit incl=30 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 str_i30ir.fit incl=30 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 gas_i30ir.fit incl=30 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 str_i30j.fit incl=30 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 gas_i30j.fit incl=30 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 str_i30jr.fit incl=30 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 gas_i30jr.fit incl=30 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 str_i30l.fit incl=30 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 gas_i30l.fit incl=30 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 str_i30lr.fit incl=30 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 gas_i30lr.fit incl=30 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 str_i30m.fit incl=30 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 gas_i30m.fit incl=30 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 str_i30mr.fit incl=30 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 gas_i30mr.fit incl=30 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 str_i60a.fit incl=60 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 gas_i60a.fit incl=60 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 str_i60ar.fit incl=60 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 gas_i60ar.fit incl=60 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 str_i60b.fit incl=60 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 gas_i60b.fit incl=60 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 str_i60br.fit incl=60 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 gas_i60br.fit incl=60 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 str_i60c.fit incl=60 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 gas_i60c.fit incl=60 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 str_i60cr.fit incl=60 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 gas_i60cr.fit incl=60 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 str_i60d.fit incl=60 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 gas_i60d.fit incl=60 prograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 str_i60dr.fit incl=60 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 gas_i60dr.fit incl=60 retrograde M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 str_i60e.fit incl=60 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 gas_i60e.fit incl=60 prograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 str_i60er.fit incl=60 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 gas_i60er.fit incl=60 retrograde M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 str_i60f.fit incl=60 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 gas_i60f.fit incl=60 prograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 str_i60fr.fit incl=60 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 gas_i60fr.fit incl=60 retrograde M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=10 str_i60g.fit incl=60 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 gas_i60g.fit incl=60 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 str_i60gr.fit incl=60 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 gas_i60gr.fit incl=60 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 str_i60h.fit incl=60 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 gas_i60h.fit incl=60 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 str_i60hr.fit incl=60 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 gas_i60hr.fit incl=60 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 str_i60i.fit incl=60 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 gas_i60i.fit incl=60 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 str_i60ir.fit incl=60 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 gas_i60ir.fit incl=60 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 str_i60j.fit incl=60 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 gas_i60j.fit incl=60 prograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 str_i60jr.fit incl=60 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 gas_i60jr.fit incl=60 retrograde M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 str_i60l.fit incl=60 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 gas_i60l.fit incl=60 prograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 str_i60lr.fit incl=60 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 gas_i60lr.fit incl=60 retrograde M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 str_i60m.fit incl=60 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 gas_i60m.fit incl=60 prograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 str_i60mr.fit incl=60 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 gas_i60mr.fit incl=60 retrograde M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 str_i89a.fit incl=89 polar M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 gas_i89a.fit incl=89 polar M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=1 str_i89b.fit incl=89 polar M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 gas_i89b.fit incl=89 polar M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=10 str_i89c.fit incl=89 polar M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 gas_i89c.fit incl=89 polar M(comp)/M(gal)=1.0 Ren/Rg=1 H/D=1 str_i89d.fit incl=89 polar M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 gas_i89d.fit incl=89 polar M(comp)/M(gal)=0.1 Ren/Rg=1 H/D=10 str_i89e.fit incl=89 polar M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 gas_i89e.fit incl=89 polar M(comp)/M(gal)=0.5 Ren/Rg=1 H/D=1 str_i89f.fit incl=89 polar M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 gas_i89f.fit incl=89 polar M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 str_i89g.fit incl=89 polar M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 gas_i89g.fit incl=89 polar M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=1 str_i89h.fit incl=89 polar M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 gas_i89h.fit incl=89 polar M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=10 str_i89i.fit incl=89 polar M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 gas_i89i.fit incl=89 polar M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=1 str_i89j.fit incl=89 polar M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 gas_i89j.fit incl=89 polar M(comp)/M(gal)=0.1 Ren/Rg=2 H/D=10 str_i89l.fit incl=89 polar M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 gas_i89l.fit incl=89 polar M(comp)/M(gal)=0.5 Ren/Rg=2 H/D=1 str_i89m.fit incl=89 polar M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 gas_i89m.fit incl=89 polar M(comp)/M(gal)=1.0 Ren/Rg=2 H/D=10 N. Paul M. Kuin NASA/NSSDC/ADC 1995 Jan 31 UNKNOWN UNKNOWN The original STARS* files contained additional separators between the images which were removed. The original files were flat ascii files, 8 8-byte floating point values per record with no separators between the images. The data were converted to fits using the IDL astronomy library (more information: Landsman@stars.gsfc.nasa.gov). VI_76.xml A Library of Theoretical Stellar Flux Spectra. I. Synthetic UBVRI photometry and the metallicity scale for F- to K-type stars 6078 VI/78 Theoretical Stellar Flux Spectra for F- to K-type Stars A Library of Theoretical Stellar Flux Spectra. I. Synthetic UBVRI photometry and the metallicity scale for F- to K-type stars R Buser R L Kurucz Astron. Astrophys. 264 557 1992 1992A&A...264..557B Models, atmosphere Stars, late-type In conjunction with Kurucz' (1979a,b) models for O to G stars, the present models for F- to K- stars provide an extensive, quasi-homogeneous grid of low-resolution theoretical flux spectra for a significant range in stellar parameters covering mostly of the observed HR diagram. The file bklate.dat contains 242 theoretical model atmosphere flux distributions for late-type stars. These flux distributions were calculated by Buser & Kurucz in 1983-5 using published and unpublished models by Gustafsson and his associates. Please refer to the publication (A&A 264, 447) for a full description of the calculations and a discussion of synthetic UBVRI photometry computed from these models. The models cover the following ranges in the parameter space: ----------------------------------------------------------- number fraction of hydrogen xH =0.9 all models turbulent velocity [km/s] vturb =2.00 234 models vturb =5.00 8 models ----------------------------------------------------------- 3750 <= Teff <= 6000 (K) 0.75 <= log.g <= 5.25 (cm/s/s) -3.00 <= [Fe/H] <= 0.50 (dex) ----------------------------------------------------------- Notice that the model sequence does NOT strictly follow an orderly pattern in parameter space, because the present file was composed from several original files having their individual parameter sequences. The last model (#242) is the solar model. Note that the present file still contains 8 models (out of a total of 242) which have turbulent velocities vturb=5.00 km/s, but whose flux distributions have n o t actually been computed for this value of vturb (=5.00 km/s). Hence, for these models, the flux distributions given in the present file are erroneous and should not be used at all. It is suggested that the user d e l e t e them from the file altogether; for the user's convenience, these models are marked on the accompanying list.
Roland Buser Astron. Inst. Basel 1995 Feb 17 buser1@urz.unibas.ch VI_78.xml ELP 2000-85: a semi-analytical lunar ephemeris adequate for historical times 6079 VI/79 Lunar Solution ELP 2000-82B ELP 2000-85: a semi-analytical lunar ephemeris adequate for historical times M Chapront-Touze J Chapront Astron. Astrophys. 190 342 1988 1988A&A...190..342C ELP 2000-85: a semi-analytical lunar ephemeris adequate for historical times M Chapront-Touze J Chapront Astron. Astrophys. 124, 50 ??? ??? 1983 1983A&A...124...50C Ephemerides Moon ephemerides celestial mechanics, stellar dynamics The theory of the lunar motion consists of the series of the semi-analytical solution ELP2000-82. The constants of the subsequent lunar ephemeris are fitted to the numerical integration DE200/LE200 of the Jet Propulsion Laboratory and the arguments come from the semi-analytical theory ELP 2000-85.
The semi-analytical lunar theory ELP 2000-82 contains purely trigonometric series and Poisson series proportional to the time (t) or the square of the time (t2). 36 data files include the series related to various components of the theory for the 3 spherical coordinates: longitude, latitude and distance. Units are arcsecond for longitude and latitude, kilometer for distance. Arguments, constants and coordinate systems are described in the notice "Lunar solution ELP 2000-82B" (elp82b.ps). All this set allows to compute a high precision lunar ephemeris. A FORTRAN example is provided (EXAMPLE) which makes use of the basic subroutine ELP82B.
elp82b.ps Postscript Notice "Lunar solution ELP 2000-82B" Gerard Francou BDL 1995 May 31 Authors' Address: M. Chapront-Touze, J. Chapront Bureau des Longitudes, CNRS URA 707 77, Avenue Denfert-Rochereau 75014, Paris, France Tel : (33) 1 40 51 22 66 (33) 1 40 51 22 71 Fax : (33) 1 46 33 28 34 VI_79.xml Opacities for stellar envelopes 6080 VI/80 Opacities from the Opacity Project Opacities for stellar envelopes M J Seaton Y Yan D Mihalas A K Pradhan Mon. Not. R. Astron. Soc. 266 805 1994 1994MNRAS.266..805S Opacities for stellar envelopes M J Seaton Mon. Not. R. Astron. Soc. 265, L25 ??? ??? 1993 1993MNRAS.265L..25S Opacities Opacities 1 CODES. ***** 1.1 Code rop.for ************ This code reads opacity files written in standard OP format. Its main purpose is to provide documentation on the contents of the files. This code, like the other codes provided, prompts for the name of the file (or files) to be read. The file names read in response to the prompt may have up to 128 characters. 1.2 Code opfit.for ************** This code reads opacity files in standard OP format, and provides for interpolation of opacities to any required values of temperature and mass-density. The method used is described in OPF. The code prompts for the name of a file giving all required control parameters. As an example, the file opfit.dat is provided (users will need to change directory names and file names). The use of opfit.for is illustrated using opfit.dat. Most users will probably want to adapt opfit.for for use as a subroutine in other codes. Timings for DEC 7000 ALPHA: 0.3 sec for data read and initialisations; then 0.0007 sec for each temperature-density point. Users who like OPAL formats should note that opfit.for has a facility to produce files of OP data in OPAL-type formats. 1.3 Code ixz.for ************ This code provides for interpolations to any required values of X and Z. See S95A. It prompts for the name of a file giving all required control parameters. An example of such a file if provided, ixz.dat (the user will need to change directory and file names). The output files have names s92INT.'nnn'. The user specifies the first value of nnn, and the number of files to be produced. 2. DATA FILES ********** 2.1 Data files for solar metal-mix ****************************** Data for solar metal-mix s92 as defined in SYMP. These files are from version 2 runs of December 1994 (see S95A for details on Version 2). There are 213 files with names s92.'nnn', 'nnn'=201 to 413. Each file occupies 83762 bytes. The file s92.version2 gives values of X (hydrogen mass-faction) and Z (metals mass-fraction) for each value of 'nnn'. The user can get s92.version2, select the values of 'nnn' required, then get the required files s92.'nnn'. The files s92.'nnn' can be used with opfit.for to obtain opacities for any requires value of temperature and mass density. Files for other metal-mixtures will be added in due course. Send requests to mjs@star.ucl.ac.uk. 2.2 Files for interpolation in X and Z ********************************** The data files have names s92xz.'mmm', where 'mmm'=001 to 096. They differ from the standard OP files (such as s92.'nnn' --- section 2.1 above) in that they contain information giving derivatives of opacities with respect to X and Z. Each file s92xz.'mmm' occupies 148241 bytes. The interpolations to any required values of X and Z are made using ixz.for. Timings: on DEC 7000 ALPHA, 2.16 sec for each new-mixture file. For interpolations to some specified values of X and Z, one requires just 4 files s92xz.'mmm'. Most users will not require the complete set of files s92xz.'mmm'. The file s92xz.index includes a table (starting on line 3) giving values, for each 'mmm' file, of x,y,z (abundances by number-factions) and X,Y,Z (abundances by mass-fractions). Users are advised to get the file s92.index, and select values of 'mmm' for files required, then get those files. The files produced by ixz.for are in standard OP format and can be used with opfit.for to obtain opacities for any required values of temperature and mass density. 3 RECOMMENDED PROCEDURE FOR USE OF OPACITY FILES ********************************************** (1) Get the file s92.version2. (2) If the values of X and Z you require are available in the files s92.'nnn' then get those files. (3) If not, get the file s92xz.index. (4) Select from s92xz.index the values of 'mmm' which cover the range of X and Z in which your are interested. Get those files and use ixz.for to generate files for your exact required values of X and Z. (5) Note that the exact abundance mixtures used are specified in each file (see rop.for). Also each run of opfit.for produces a table of abundances. (6) If you want a metal-mix different from that of s92, contact mjs@star.ucl.ac.uk. 4 FUTURE DEVELOPMENTS ******************* (1) Files will be added very shortly for calculation of radiative forces. (2) Facilities will be added later which will enable the user to make calculations giving files for any required mixtures.
Summary of solar metal-mix s92 data Version Version designation "OP Version 2.0 S92" --- Mix Mixture number --- text1 "X=" --- X Hydrogen mass-fraction --- text2 ", Z=" --- Z Metal (Z>=3) mass-fraction --- Date Computation date --- Mike J. Seaton Univ. Coll. London 1995 Apr 18 VI_80.xml Planetary Theories in rectangular and spherical variables: VSOP87 solution. 6081 VI/81 Planetary Solutions VSOP87 Planetary Theories in rectangular and spherical variables: VSOP87 solution. P Bretagnon G Francou Astron. Astrophys. 202 309 1988 1988A&A...202..309B Planetary Theories in rectangular and spherical variables: VSOP87 solution. P Bretagnon Astron. Astrophys. 114 278 1982 1982A&A...114..278B VI/88 : Ephemerides of Pluto based on DE200 (Chapront+ 1995) VI/87 : Planetary Ephemerides based on DE403 (Chapront+ 1996) Ephemerides planets and satellites: general ephemerides celestial mechanics, stellar dynamics The Planetary solutions VSOP87 (Variations Seculaires des Orbites Planetaires) are analytical solutions of the motion of the planets in different versions. The main version VSOP87 consists of the series in elliptic elements as in the case of VSOP82 solution and the other versions VSOP87 (A-B-C-D-E) are built in in rectangular and spherical variables.
The main version of VSOP87 is similar to the previous theory VSOP82. In the both cases the constants of integration have been determined by fitting to the numerical integration DE200 of the Jet Propulsion Laboratory. The various versions of VSOP87 are different from one to another in the type of coordinates and the reference frame. VSOP87 : heliocentric elliptic variables; equinox and ecliptic J2000. VSOP87A : heliocentric rectangular variables; equinox and ecliptic J2000. VSOP87B : heliocentric spherical variables; equinox and ecliptic J2000. VSOP87C : heliocentric rectangular variables; equinox and ecliptic of date. VSOP87D : heliocentric spherical variables; equinox and ecliptic of date. VSOP87E : barycentric rectangular variables; equinox and ecliptic J2000. A program EXAMPLE (Fortran 77) is provided which makes use of the subroutine VSOP87 which substitutes the time in the series of the solutions VSOP87.
vsop87.doc Notice for use of VSOP87 files Gerard Francou BDL Francois Ochsenbein CDS 1995 May 31 Authors' Address: P. Bretagnon, G. Francou Bureau des Longitudes, CNRS URA 707 77, Avenue Denfert-Rochereau 75014, Paris, France Tel : (33) 1 40 51 22 69 (33) 1 40 51 22 60 Fax : (33) 1 46 33 28 34 E-mail : pierre@bdl.fr francou@bdl.fr VI_81.xml High Resolution Absorption Cross-section Measurements of Ozone at 195 K in the Wavelength Region 240-350 nm 6083 VI/83 O3 and SO2 Absorption Cross Sections High Resolution Absorption Cross-section Measurements of Ozone at 195 K in the Wavelength Region 240-350 nm D E Freeman K Yoshino J R Esmond W H Parkinson Planetary Sp. Sci. 32 2: 239-248, ??? ??? 1984 1984 High Resolution Absorption Cross-section Measurements of Ozone at 195 K in the Wavelength Region 240-350 nm K Yoshino D E Freeman J R Esmond W H Parkinson Planetary. Sp. Sci., 36 4: 395-398, ??? ??? 1988 1988 High Resolution Absorption Cross-section Measurements of Ozone at 195 K in the Wavelength Region 240-350 nm K Yoshino J R Esmond D E Freeman W H Parkinson J. Geophys. Res., March 20 98 D3: 5205-5211 ??? ??? 1993 1993 High Resolution Absorption Cross-section Measurements of Ozone at 195 K in the Wavelength Region 240-350 nm D E Freeman Y Yoshino J R Esmond W H Parkinson Planetary Sp. Sci. 32 1125-1134 1984 1984 Atomic physics Spectroscopy Cross sections Cross sections of the Hartley-Huggins bands of O3 at the temperature 195K were obtained from photoabsorption measurements at column densities in the range 2 x 10^17 - 1 x 10^21 cm-2 throughout the wavelength region 240-350 nm. Measurements of the absolute absorption cross-section of ozone at the temperatures 195, 228 and 295 K were made at several discrete wavelengths in the region 238-335 nm and measurements of the relative absorption cross sections were made temperatures 195, 228 and 295 K throughout the wavelength region 185-254 nm. Laboratory measurements at high resolution of the absorption cross section of SO2 at the temperature 213 K in the wavelength region 172-240 nm are also given.
O3: Cross sections of the Hartley-Huggins bands of O3 at the temperature 195 K were obtained from photoabsorption measurements at column densities in the range 2 x 10^17 - 1 x 10^21 cm-2 throughout the wavelength region 240-350 nm with a 6.65 m photoelectric scanning spectrometer equipped with a 2400 lines mm-1 grating and operated at an instrumental width (FWHM) of 0.003 nm. These were published in 1984. The cross sections were later put on a different absolute basis reflecting the absolute cross section measurements at discrete points of ozone at three different temperatures, published in 1988 (Planetary Space Science, 36(4): 395-398). The files available here reflect this recalibration. Laboratory measurements of the absolute absorption cross-section of ozone at the temperatures 195, 228 and 295 K were made at several discrete wavelengths in the region 238-335 nm. The results for ozone at 295 K are in excellent agreement with those of Hearn (1961, Proc. phys. Soc. Lond., 78, 932), who used a different technique. Their absolute cross-section measurements of ozone at 195 K have been used by the authors to put their recent relative cross-section measurements at that temperature (Freeman et al., 1984, Planet. Space Sci., 32, 239) on a firm absolute basis throughout the region 240-335 nm; Laboratory measurements of the relative absorption cross sections of ozone at the temperatures 195, 228 and 295 K were made throughout the wavelength region 185-254 nm. The absolute absorption cross sections at the same temperatures were measured at several discrete wavelengths in the region 185-254 nm. The absolute cross sections of ozone were used to put relative cross sections on a firm absolute basis throughout the region 185-255 nm. These recalibrated cross sections below 250 nm are slightly lower than those of Molina and Molina (J. Geophys. Res., 91, 14501 (1986) ), but differences are within a few percent and would not be significant in atmospheric applications. These later measured cross sections supersede the earlier high resolution measurements published (Planet. Space Sci., 32(2): 239-248, (1984); and Planet. Space Sci., 36(4): 395-398, (1988) ) in the region where they overlap. SO2: Laboratory measurements at high resolution of the absorption cross section of SO2 at the temperature 213 K were made in the wavelength region 172-240 nm with a 6.65 m scanning spectrometer/ spectrograph operated at an instrumental width of 0.002 nm. The measured cross sections are presented graphically in representative wavelength regions and are available throughout the region 172-240 nm at wavenumber intervals of 0.4-0.1 cm-1 The measured cross sections, which are relevant to the photochemistry of planetary atmospheres, possess significantly more spectroscopic structure, and are more accurate, than previous measurements made at lower resolution.
sulfur dioxide cross sections Ozone cross sections at 213K Ozone cross sections at 195K Ozone cross sections at 228K Ozone cross sections at 295K nu Wavenumber position, cm-1 sigma Cross section/molecule --- Nancy G. Roman ADC/SSDOO 1995 Oct 04 We thank Dr. Yoshino and Jim Esmond for forwarding the files to us. We also thank Mr. Esmond for reviewing our original document, providing corrections and substantial additional information, and replacing a data file which had been received in garbled form. VI_83.xml Identification List of Lines in Stellar Spectra in the Ultraviolet region (UVILLSS Catalogue) 6084 VI/84 UVILLSS Catalogue Identification List of Lines in Stellar Spectra in the Ultraviolet region (UVILLSS Catalogue) R Coluzzi Bull. Inf. CDS 48 15 1996 1996BICDS..48...15C Atomic physics Spectra, ultraviolet This catalogue is an extension in the ultraviolet region (129 to 3903 Angstroems) of the ILLSS catalogue (Coluzzi, 1993; catalog <VI/71>) which lists lines in the optical region. The data are from "Ultraviolet Multiplet Table" (Moore 1950, 1952, 1962) and arranged in two files: the catalogue and the references. There are two versions of each file, one presented in the author's original format, and the second organised as a table. The reference files are arranged by element: for each spectrum the first line contains within parenthesis the Ionization Potential; the grade of analysis; the grade denoting the relative number of classified lines included as compared with the total number classified in the ultraviolet; the date of completion of the manuscript; the limit for three spectra H, He I, He II. The limit in cm-1 has been multiplied by the factor 0.00012345 to obtain the tabulated ionisation potential, which is expressed in electron-Volts. The analysis grades range from A to E, grade A indicating that the analysis is essentially complete ,and grade E that the structure has been recognised, but is limited to a single multiplet or transition. List A, List B, etc., denote the relative numbers of classified lines listed here as compared with the total number classified in the ultraviolet, A denoting that all classified lines in the ultraviolet are listed, and D that only a few of the leading ones are tabulated. The letters on the left, A, B, C, etc. preceding the reference, indicate the source used for the wavelength quoted in the Table. Those papers used only for analysis or intensity follow the ones used for wavelength, and are not preceded by the letters denoting the source. The letters "WL", "I", "T", indicating what was taken from each paper for the Table compilation , denote, respectively, wavelength, intensity, and terms, the last referring to the analysis of the spectrum. These informations are taken from Moore (1950).
The catalogue as a formatted table lambda Wavelength in Angstroems 0.1nm Element Element name and spectrum --- Z Atomic element number --- Ion Electronic charge --- n_lambda '*' for blend, 'a' for air lambda --- Multiplet Multiplet number --- RefL Reference of intensity number=1 the Element, associated to the reference letter RefL, is the key to retrieve the reference in file refs.dat --- Intens Intensity with Moore notation number=2 the following notations are used: - A colon : indicates that the intensity is not the first or second choice (in place of the original parentheses) - The letters have the following meaning: 'bl' blended 'd' double 'g' ghost 'l' shaded to longer wave-length 'n' diffuse or hazy 'N' very diffuse or very hazy 'p' part of band 'r' narrow self-reversal 'R' wide self-reversal 's' shaded to shorter wave-length 'tr' trace 'w' wide(fine structure type),broad or complex 'W' very wide(fine structure type) or very broad --- n_Intens Notes about the Intensity number=2 the following notations are used: - A colon : indicates that the intensity is not the first or second choice (in place of the original parentheses) - The letters have the following meaning: 'bl' blended 'd' double 'g' ghost 'l' shaded to longer wave-length 'n' diffuse or hazy 'N' very diffuse or very hazy 'p' part of band 'r' narrow self-reversal 'R' wide self-reversal 's' shaded to shorter wave-length 'tr' trace 'w' wide(fine structure type),broad or complex 'W' very wide(fine structure type) or very broad --- IP Ionisation Potential eV u_IP Uncertainty note on IP --- References as a formatted table Element Element name and spectrum number=1 the Element, associated to the reference letter RefL, is the key to retrieve the reference in file refs.dat --- RefL Reference in element number=1 the Element, associated to the reference letter RefL, is the key to retrieve the reference in file refs.dat --- Text of reference --- uvillss.ref *The UVILLSS finding list this is the file as described in the publication. Francois Ochsenbein CDS 1997 Mar 27 Regina Coluzzi <coluzzi@coma.mporzio.astro.it> UNKNOWN UNKNOWN * 03-Apr-1996: First version * 28-Mar-1997: The Intens column which was stored as characters, have been transformed into a numeric intensity plus a remarks column at CDS (F. Ochsenbein). The very high value of 100000 for the line at 1178.650Angstroems was then changed to 99999. VI_84.xml Bibliography of Atomic Line Identification Lists 6086 VI/86 Bibliography of Atomic Line Identification Lists Bibliography of Atomic Line Identification Lists S J Adelman Pub. Astron. Soc. Pacific 108 633 1996 1996PASP..108..633A Bibliography of Atomic Line Identification Lists S J Adelman M A J Snijders Pub. Astron. Soc. Pacific 86 1018 1974 1974PASP...86.1018A Bibliography of Atomic Line Identification Lists S J Adelman Pub. Astron. Soc. Pacific 90 766 1978 1978PASP...90..766A Bibliography of Atomic Line Identification Lists S J Adelman Pub. Astron. Soc. Pacific 95 897 1983 1983PASP...95..897A Bibliography of Atomic Line Identification Lists S J Adelman Pub. Astron. Soc. Pacific 101 302 1989 1989PASP..101..302A Bibliography Catalogs Atomic and molecular data Adelman and Snijders (1974) compiled a bibliography of atomic line identification lists to supplement the data contained in the Ultraviolet and Revised Multiplet Tables (Moore 1945, 1950, 1952, 1962) and Kelly and Palumbo (1973) for the wavelength region 911-8250 Angstroms and the first four spectra of all elements. Four supplements (Adelman 1978, 1983, 1989, 1996) also included references to the fifth and sixth spectra of key elements through the iron peak. The table lists references found in the these papers except for those which have been superseded by more recent compilations. Each entry indicates the wavelength region covered in Angstroms unless otherwise noted and the type of reference: A = analysis, AW = very accurate wavelengths, CL = classified lines, EA = extension of analysis, IS = isotopic shifts, NMT = new multiplet table, RA = revised analysis, TC = temperature classification, and W = wavelength list. The reader is advised to examine each reference to determine its quality.
Bibliography of atomic line data ID Identification of atomic or ionic species If ID is a blank field, the reference information is a continuation of the previous record. --- Ref Reference --- C.-H. Joseph Lyu Hughes STX/NASA 1997 Jan 27 Saul J. Adelman, Department of Physics, The Citadel 171 Moultrie Street, Charleston, SC 29409 Electronic mail: adelmans@citadel.edu UNKNOWN UNKNOWN Gallagher (1993) edited C. E. Moore's Tables of Spectra of Hydrogen, Carbon, Nitrogen, and Oxygen Atoms, most of which were published as part of NSRDS-NBS 3. This work was supported in part by grants from " The Citadel Development Foundation." VI_86.xml Ephemerides of planets between 1900 and 2100 (1998 update) 6087 VI/87 Planetary Ephemerides Ephemerides of planets between 1900 and 2100 (1998 update) J Chapront G Francou Bureau des Longitudes, Group : Dynamics of Solar System ??? ??? 1996 1986 VI/66 : Precession Formulae and Mean Elements for Moon and Planets (Simon et al., 1994) VI/79 : Lunar Solution ELP 2000-82B (Chapront-Touze+, 1988) VI/81 : Planetary Solutions VSOP87 (Bretagnon+, 1988) VI/88 : Ephemerides of Pluto based on DE200 (Chapront+ 1995) J/A+AS/109/181 : Ephemerides of outer planets (Chapront 1995) Bretagnon P., Francou G., 1988, A&A 202, 309 (1988A&A...202..309B) Chapront J., 1995, A&AS 109, 181 (1995A&AS..109..181C) Simon J.L., Bretagnon P., Chapront J., Chapront-Touze M., Francou G., Laskar J., 1994, A&A 282, 663 (1994A&A...282..663S) Ephemerides Planets planets ephemerides celestial mechanics, stellar dynamics Planetary motions have been represented with series resulting of an approximation by frequency analysis of JPL numerical integration DE403. Series represent the heliocentric coordinates of planets as functions of time between 1900 and 2100 for the 9 bodies : Mercury, Venus, Earth-Moon Barycenter, Mars, Jupiter, Saturn, Uranus, Neptune and Pluto. The method allows to compute planetary ephemerides with the aid of compact tables and keeps accuracy of published ephemerides.
The presentation of the series is given in file series96.doc. The planetary series are in files series96.xxx (one file per planet). A Fortran subroutine series96.sub (96.12) uses the series for computing the heliocentric rectangular coordinates of planets. A Fortran program series96.f is provided to illustrate the use of the series in the case of the computation of astrometric coordinates. An executable DOS program, planeph.exe, allows to compute the most usual planetary ephemerides with the series between 1900 to 2100. The file planeph.doc gives explanations for using this program with the data sets planeph.tab and planeph.loc.
series96.doc Notice for the use of the series. planeph.doc Notice for the use of the program planeph.exe G. Francou BDL F. Ochsenbein CDS 1998 Oct 07 Authors' Addresses: J. Chapront, Observatoire de Paris DANOF 61, avenue de l'Observatoire - F75014 PARIS E-mail : jchapron@danof.obspm.fr G. Francou, Observatoire de Paris Institut de mecanique celeste et de calcul des ephemerides 77, avenue Denfert-Rochereau - F75014 PARIS E-mail : francou@bdl.fr UNKNOWN UNKNOWN * 28-Jan-1997: first version * 07-Oct-1998: installation of 1998 update, replacement of the planeph.exe by the newer version (4.2). No change occured in the data files. VI_87.xml Ephemerides of Pluto between 1700 and 2100 (PLUTO95) 6088 VI/88 Ephemerides of Pluto Ephemerides of Pluto between 1700 and 2100 (PLUTO95) J Chapront G Francou Bureau des Longitudes, Group : Dynamics of Solar System ??? ??? 1995 1995 VI/81 : Planetary Solutions VSOP87 (Bretagnon+, 1988) VI/87 : Planetary Ephemerides based on DE403 (Chapront+ 1996) Chapront J., 1995, A&AS 109, 181 (1995A&AS..109..181C) Ephemerides planets and satellites: general ephemerides celestial mechanics, stellar dynamics Pluto's motion has been represented with series resulting of an approximation by frequency analysis (see Chapront 1995) of JPL numerical integration DE200. Series represent the heliocentric coordinates of Pluto as functions of time between 1700 and 2100. This catalog completes the VSOP87 theories developed at the Bureau des Longitudes (see Cat. <VI/81>)
The presentation of the tables is given in file : pluto.doc. A Fortran subroutine pluto.sub (95.1) is provided for the computation of the heliocentric rectangular positions and velocities of Pluto.
pluto.doc Notice for usage Gerard Francou BDL 1997 Jan 28 J. Chapront, G. Francou Bureau des Longitudes Group : Dynamics of Solar System 77, avenue Denfert-Rochereau F-75014 Paris - France E-mail : jchapron@bdl.fr francou@bdl.fr Phone : (33) 1 40 51 22 71 (33) 1 40 51 22 60 Fax : (33) 1 46 33 28 34 VI_88.xml Opacities for stellar envelopes 6089 VI/89 Radiative forces for stellar envelopes Opacities for stellar envelopes M J Seaton Y Yan D Mihalas A K Pradhan Mon. Not. R. Astron. Soc. 266 805 1994 1994MNRAS.266..805S Opacities for stellar envelopes M J Seaton Mon. Not. R. Astron. Soc. 265, L25 ??? ??? 1993 1993MNRAS.265L..25S Opacities for stellar envelopes M J Seaton Mon. Not. R. Astron. Soc. 279 95 1996 1996MNRAS.279...95S Opacities for stellar envelopes M J Seaton Mon. Not. R. Astron. Soc. 289 700 1997 1997MNRAS.289..700S VI/80 : Opacities from the Opacity Project (Seaton+, 1995) Opacities from the Opacity Project. For general description see M.J. Seaton, Yu Yan, D. Mihalas and Anil K. Pradhan, 1994MNRAS.266..805S . This paper will be referred to as SYMP. For interpolation of opacities as functions of temperature and density see M.J. Seaton, 1993MNRAS.265L..25S . This paper will be referred to as OPF. For interpolations of opacities as functions of X (hydrogen mass- fraction) and Z (metals mass-fraction), for fixed relative abundances of metal atoms, see M.J. Seaton, 1996MNRAS.279...95S . This paper will be referred to as IXZ. For the calculation of forces on atoms of individual elements due to radiation pressure, calculated using atomic data from the Opacity Project. see M.J. Seaton, 1997MNRAS.289..700S This paper will be referred to as ACC. Atomic physics Models, atmosphere stars: opacities stars: radiative accelerations stars: stellar envelopes stars: diffusion (1) Primary data files, stages.zz These files give data for the calculation of radiative accelerations, GRAD, for elements with nuclear charge zz. Data are available for zz=06, 07, 08, 10, 11, 12, 13, 14, 16, 18, 20, 24, 25, 26 and 28. Calculations are made using data from the Opacity Project (see papers SYMP and IXZ). The data are given for each ionisation stage, j. They are tabulated on a mesh of (T, Ne, CHI) where T is temperature, Ne electron density and CHI is abundance multiplier. The files include data for ionisation fractions, for each (T, Ne). The file contents are described in the paper ACC and as comments in the code add.f (2) Code add.f This reads a file stages.zz and creates a file acc.zz giving radiative accelerations averaged over ionisation stages. The code prompts for names of input and output files. The code, as provided, gives equal weights (as defined in the paper ACC) to all stages. Th weights are set in SUBROUTINE WEIGHTS, which could be changed to give any weights preferred by the user. The dependence of diffusion coefficients on ionisation stage is given by a function ZET, which is defined in SUBROUTINE ZETA. The expressions used for ZET are as given in the paper. The user can change that subroutine if other expressions are preferred. The output file contains values, ZETBAR, of ZET, averaged over ionisation stages. (3) Files acc.zz Radiative accelerations computed using add.f as provided. The user will need to run the code add.f only if it is required to change the subroutines WEIGHTS or ZETA. The contents of the files acc.zz are described in the paper ACC and in comments contained in the code add.f. (4) Code accfit.f This code gives gives radiative accelerations, and some related data, for a stellar model. Methods used to interpolate data to the values of (T, RHO) for the stellar model are based on those used in the code opfit.for (see the paper OPF). The executable file accfit.com runs accfit.f. It uses a list of files given in accfit.files (see that file for further description). The mesh used for the abundance-multiplier CHI on the output file will generally be finer than that used in the input files acc.zz. The mesh to be used is specified on a file chi.dat. For a test run, the stellar model used is given in the file 10000_4.2 (Teff=10000 K, LOG10(g)=4.2) The output file from that test run is acc_10000_4.2. The contents of the output file are described in the paper ACC and as comments in the code accfit.f. (5) The code diff.f This code reads the output file (e.g. acc_100000_4.2) created by accfit.f. For any specified depth point in the model and value of CHI, it gives values of radiative accelerations, the quantity ZETBAR required for calculation of diffusion coefficients, and Rosseland-mean opacities. The code prompts for input data. It creates a file recording all data calculated. The code diff.f is intended for incorporation, as a set of subroutines, in codes for diffusion calculations.
Mike J. Seaton Univ. Coll. London 1997 Aug 08 Author's address: Mike J. Seaton, University College London Email: mjs@star.ucl.ac.uk VI_89.xml Wide-Field Plate Database 6090 VI/90 Wide-Field Plate Database Wide-Field Plate Database M K Tsvetkov K Y Stavrev K P Tsvetkova A S Mutafov E H Semkov Institute of Astronomy, Bulgarian Academy of Sciences ??? ??? 1997 1997 Atlases Plate data Observatory log Photographic catalog The Wide-Field Plate Database (WFPDB) contains the descriptive information for the astronomical wide-field (~>1deg.) photographic observations stored in numerous archives all over the world. When finished it will provide an on-line access to the information for about 2 million observations from nearly 300 archives, obtained since the end of last century. Presently the WFPDB includes data for about 330 000 observations from 57 plate catalogues. About 120 000 observations more from 32 plate catalogs are in preparation to be included in the database. The WFPDB provides for each observation information for the corresponding archive, the parameters of the observational instrument, the observation parameters (position on sky, observation time, object name, method, exposure time, emulsion type, filter type, spectral band, plate size), as well as data on the plate quality, comments, and observers. Data on the plate availability and digitization will be supplemented in the WFPDB in the future.
List of plate archives IDobs WFPDB observatory identifier Fields from byte 1 to byte 7, taken together, constitute the WFPDB instrument identifier. --- IDins Instrument aperture cm IDsuf1 Suffix to the instrument identifier --- LOCs Location of the plate archive, town (site) --- LOCc Location of the plate archive, country --- OBSn Observatory, name --- OBSs Observatory, site --- OBSc Observatory, country --- MNo Marsden's number --- TZ- Time zone, sign --- TZ Time zone h LON- Observatory longitude, sign --- LONd Observatory longitude, deg deg LONm Observatory longitude, arcmin arcmin LAT- Observatory latitude, sign --- LATd Observatory latitude, deg deg LATm Observatory latitude, arcmin arcmin ALT Observatory altitude m MULT Multiplicity of telescope cameras --- --- Sign 'x' --- APR Clear aperture of the telescope m MD Diameter of telescope mirror m FL Focal length of the telescope m SCL Plate scale arcsec/mm ITYPE Instrument type Ast - astrograph, Cam - camera, FEC - fish eye camera, Men - meniscus, RCr - Ritchey-Chretien, Rfl - reflector, Rfr - refractor, Sch - Schmidt --- FIELD Field angular dimension deg YEAR1 Year of beginning of telescope operation yr YEAR2 Year of end of telescope operation yr PF Indication 'F' for 'film' --- NPd Number of direct plates --- NPUNd Uncertainty of the number of plates --- CFORMd Plate catalog form (direct plates) C - computer-readable form, T - printed table form, TC - computer-readable form in preparation --- NPs Number of objective prism plates --- NPUNs Uncertainty of the number of plates --- CFORMs Plate catalog form (obj. prism plates) --- QUAL Code for quality of the plate archive A - very good, B - good, D - distributed --- ANAME Astronomer in charge --- Main data file IDobs WFPDB observatory identifier Fields from byte 1 to byte 14, taken together, constitute the WFPDB plate identifier. Fields from byte 1 to byte 7 constitute the WFPDB instrument identifier. --- IDins Instrument aperture cm IDsuf1 Suffix to the instrument identifier --- IDno Original plate number --- IDsuf2 Suffix to the original plate number --- RAh Right ascension (hours) (J2000.0) h RAm Right ascension (minutes) min RAs Right ascension (seconds) s DE- Declination sign (J2000.0) --- DEd Declination, degrees deg DEm Declination, arcminutes arcmin DEs Declination, arcseconds arcsec CCOD Code for Error, Missing data, or Uncertainty of coordinates --- DATEy Date of observation, year (UT) yr DATEm Date of observation, month month DATEd Date of observation, day d UTh Observation time (hour) (UT) h UTm Observation time (min) min UTs Observation time (sec) s TCOD Code for Error, Missing data, or Uncertainty of observation time --- OBJNAM Object or field designation --- OBJTYP Object type code Object type in WFPDB is coded as follows: A1 - planet A2 - moon A3 - sun A4 - asteroid A5 - comet S1 - star S2 - double star S3 - variable star S4 - star cluster S5 - HII region S6 - nebula S7 - planetary nebula S8 - supernova S9 - fundamental star SR - reference star around a radio source G1 - galaxy G2 - QSO G3 - group of galaxies G4 - cluster of galaxies G5 - supercluster G6 - void F - field Remark: Object type for most of the observations is not yet available in the WFPDB. --- METHOD Method of observation code Method of observation in WFPDB is coded as follows: 1 - direct photograph 2 - direct photograph, multiexposure 3 - stellar tracks 4 - objective prism 5 - objective prism, multiexposure 6 - Metcalf's method 7 - proper motions 8 - no guiding 9 - out of focus 10 - test plate 11 - Hartmann test 12 - with mask 14 - sub-beam (Pickering) prism 24 - objective grating --- MULTEX Multiplicity of exposure --- EXP Exposure time For multiexposures with different duration of the separate exposures the 2nd, 3rd, ... exposures are given in file 'notes', if available in the original plate catalogs. min EMULS Emulsion type --- FILT Filter type --- SPEC Spectral band --- DIMx X dimension of plate cm DIMy Y dimension of plate cm PQUAL Pointer to file 'quality' --- PNOT Pointer to file 'notes' --- POBS Pointer to file 'observer' --- PAVA Pointer to file 'availability' Files 'availability' and 'digitisation' are not available. --- PDIG Pointer to file 'digitisation' --- Plate quality data IDobs WFPDB observatory identifier See notes to description of file 'maindata'. --- IDins Instrument aperture cm IDsuf1 Suffix to the instrument identifier --- IDno Original plate number --- IDsuf2 Suffix to the original plate number --- CONT Continuation sign (1, 2, ...) or blank --- QTEXT Text of quality information --- Notes IDobs WFPDB observatory identifier See notes to the description of file 'maindata'. --- IDins Instrument aperture cm IDsuf1 Suffix to the instrument identifier --- IDno Original plate number --- IDsuf2 Suffix to the original plate number --- CONT Continuation sign (1, 2, ...) or blank --- NTEXT Text of note --- Observers' names IDobs WFPDB observatory identifier See notes to the description of file 'maindata'. --- IDins Instrument aperture cm IDsuf1 Suffix to the instrument identifier --- IDno Original plate number --- IDsuf2 Suffix to the original plate number --- CONT Continuation sign (1, 2, ...) or blank --- OBSNAM Observer's name(s) --- CDS 1997 May 15 Author's address: Dr. Milcho Tsvetkov E-mail, Internet: Project Manager tsvetkov@wfpa.acad.bg Wide-Field Plates Database tsvetkov@bgcict.acad.bg VI_90.xml Catalog of Solar and Lunar Eclipses: 1996-2020 A.D. 6097 VI/97 Solar and Lunar Eclipses: 1996-2020 Catalog of Solar and Lunar Eclipses: 1996-2020 A.D. F Espenak Bull. Inf. CDS in press ??? ??? 1999 1999 http://sunearth.gsfc.nasa.gov/eclipse/eclipse.htmlEspenak, F. 1989, Fifty Year Canon of Lunar Eclipses: 1986 - 2035, NASA Reference Publication 1216 Espenak F. 1987. Fifty Year Canon of Solar Eclipses: 1986 - 2035, NASA Reference Publication 1178 (1987) van den Bergh, G. 1955, Periodicity and Variation of Solar (and Lunar) Eclipses, Tjeenk Willink, Haarlem, Netherlands Sun Solar system Solar Eclipses - During the twenty-five year period 1996-2020, some portion of the Moon's shadow will sweep across the Earth a total of fifty-six times. Twenty-one of these events result in partial solar eclipses, seventeen of them are annular eclipses, sixteen more are total eclipses and the remaining two are both annular and total along sections of their narrow paths. Local circumstances at the instant of greatest eclipse1 for every event during this quarter century period are presented in solar.dat. The date and Universal Time of the instant of greatest eclipse are found in the first two columns. The eclipse type is given (T=Total, A=Annular, AT=Annular/Total or P=Partial) along with the Saros series, as defined by van den Bergh (1955). The magnitude of the eclipse is defined as the fraction of the Sun's diameter obscured at greatest eclipse. The latitude and longitude of the umbra are given for the instant of greatest eclipse, along with the Sun's altitude, the width of the path (kilometers) and the duration of totality or annularity. For partial eclipses, the latitude and longitude of the point closest to the umbra's axis at the instant of greatest eclipse are listed. The altitude of the Sun at this location is 0 degrees. Note: Greatest eclipse is defined as the instant when the axis of the Moon's shadow passes closest to the Earth's center. For total eclipses, the instant of greatest eclipse is virtually identical to the instants of greatest magnitude and greatest duration. However, for annular eclipses, the instant of greatest duration may occur at either the time of greatest eclipse or near the sunrise and sunset points of the eclipse path. Lunar Eclipses - During the twenty-five year period 1996-2020, the Moon will swing through some portion of Earth's shadow a total of fifty-eight times. Twenty-three of these events result in penumbral lunar eclipses, twelve of them are partial (umbral) eclipses, twenty-three more are total lunar eclipses. Local circumstances at the instant of greatest eclipse1 for every event during this quarter century period are presented in Table 1. The date and Universal Time of the instant of greatest eclipse are found in the first two columns. The eclipse type is given (T=Total, P=Partial [Umbral], or P=Penumbral) along with the Saros series, as defined by van den Bergh (1955). The penumbral and umbral magnitudes of the eclipse are defined as the fraction of the Moon's diameter obscured by either shadow at greatest eclipse. The partial and total semi-durations of the eclipse along with the Greenwich Siderial Time at midnight, and the Moon's Right Ascension and Declination are listed. The start and end times of the partial eclipse can be calculated by respectively subtracting and adding the partial semi-duration (i.e. - Par. SDur) to the instant of greatest eclipse. Likewise, the start and end times of the total eclipse can be calculated by respectively subtracting and adding the total semi-duration (i.e. - Total SDur) to the instant of greatest eclipse. Note: Greatest eclipse is defined as the instant when the Moon passes closest to the axis of Earth's shadow(s). This marks the instant when the Moon is deepest in Earth's shadow(s).
Solar: Local Circumstances at Greatest Eclipse Year Calendar Year (Gregorian) at instant of Greatest Eclipse yr Month Calendar Month (Gregorian) at instant of Greatest Eclipse --- Day Calendar Day (Gregorian) at instant of Greatest Eclipse d Hour Hour (UT) of Greatest Eclipse h colon Hour/Minute separator --- Minute Minute of hour of Greatest Eclipse min Type Type of eclipse Type of eclipse where: T = Total Eclipse A = Annular Eclipse AT = Annular/Total Eclipse P = Partial Eclipse --- Saros Saros series of eclipse --- Gamma Distance of the shadow cone axis from the center of Earth (units of equatorial radii) --- Magnitude Fraction of Sun's diameter obscured by Moon --- Lat Latitude where greatest eclipse is seen deg LatHemi Latitude hemisphere (North or South) --- Long Longitude where greatest eclipse is seen deg LongHemi Longitude hemisphere (East or West) --- Alt Sun's altitude at greatest eclipse deg Width Width of the path of totality or annularity at greatest eclipse km DurMin Central duration of total or annular phase at greatest eclipse (minutes) min m Minutes label --- DurSec Central duration of total or annular phase at greatest eclipse (seconds) s s Seconds label --- Lunar: Local Circumstances at Greatest Eclipse Year Calendar Year (Gregorian) at instant of Greatest Eclipse yr Month Calendar Month (Gregorian) at instant of Greatest Eclipse --- Day Calendar Day (Gregorian) at instant of Greatest Eclipse d Hour Hour (UT) of Greatest Eclipse h colon Hour/Minute separator --- Minute Minute of hour of Greatest Eclipse min Type Type of eclipse T = Total Eclipse U = Partial (Umbral) Eclipse P = Penumbral Eclipse --- n_Type Note on type "m" = Middle eclipse of Saros series "+" = Central eclipse (Moon north of axis) "-" = Central eclipse (Moon south of axis) b = first penumbral eclipse of a new saros series ("b" = beginning) c = central total eclipse (Tc) --- Saros Saros series of eclipse --- Gamma Distance of Moon from the axis of Earth's shadow cone (units of equatorial radii) --- PenMag Fraction of Moon's diameter obscured by the penumbra --- UmbMag Fraction of Moon's diameter obscured by the umbra --- ParSDur Semi-duration of partial (umbral) eclipse min mP Minutes label --- TotSDur Semi-duration of total (umbral) eclipse min mT Minutes label --- GSTO Greenwich Siderial Time at 00:00 U.T. h RA Geocentric Right Ascension of the Moon at greatest eclipse h Dec Geocentric Declination of the Moon at greatest eclipse deg James E. Gass ADC/SSDOO 1998 May 12 UNKNOWN UNKNOWN 03-Apr-1998: Data and documentation were copied from the author's web site. The data tables were modified slightly to meet CDS/ADC standard practice (e.g., deleted header and spacer records). UNKNOWN UNKNOWN Notes: The altitude 'a' and azimuth 'A' of the Moon during any phase of an eclipse depends on the time and the observer's geographic coordinates. Neglecting the effects of atmospheric refraction and lunar parallax, 'a' and 'A' are calculated as follows: h = 15 (GST0 + UT - ra) + l a = ArcSin [Sin d Sin f + Cos d Cos h Cos f] A = ArcTan [- (Cos d Sin h) / (Sin d Cos f - Cos d Cos h Sin f)] where: h = Hour Angle of Sun or Moon a = Altitude A = Azimuth GST0 = Greenwich Sidereal Time at 0:00 UT UT = Universal Time ra = Right Ascension of Sun or Moon d = Declination of Sun or Moon l = Observer's Longitude (East +, West -) f = Observer's Latitude (North +, South -) VI_97.xml Revised New General Catalogue of Nonstellar Astronomical Objects 7001B VII/1B Revised New General Catalogue Revised New General Catalogue of Nonstellar Astronomical Objects J W Sulentic W G Tifft Univ. of Arizona Press ??? ??? 1973 1973rncn.book.....S VII/13 : Arp's globular cluster catalog VII/49 : Zwicky's Catalogue of Galaxies and Clusters of Galaxies (CGCG) VII/62 : Vorontsov-Velyaminov's Morphological Catalog of Galaxies (MCG) Dreyer, J.L.E. 1888,"New General Catalogue of Nebulae and Clusters of Stars", MNRAS, 49, Part I (reprinted 1962, London: Royal Astronomical Society) Nonstellar objects Galaxy catalogs The catalog is a modern, revised, and expanded version of the original NGC (Dreyer 1888). In addition to incorporating the many corrections to the NGC found over the years, each object was verified on Palomar Observatory Sky Survey (POSS) prints and on plates for southern objects specifically taken for the purpose (although about 90 southern objects could not be verified). Please refer to the documentation by Wayne H. Warren Jr. in file "adc.doc".
The Revised NGC Catalog NGC The original NGC number --- m_NGC Component of NGC number=6 Some anonymous objects near NGC objects or components in multiple systems are assigned the same NGC number followed by a letter in alphabetic sequence --- Type Type of object number=1 the object type is coded as follows : 1 Open Cluster 6 Cluster associated with nebulosity 2 Globular Cluster 7 Non existent 3 Diffuse Nebula 8 Object in Large Magellanic Cloud 4 Planetary Nebula 9 Object in Small Magellanic Cloud 5 Galaxy 0 Unverified southern object Combination of two type numbers may appear for an object (such as 28 for a Globular cluster in LMC, etc) --- RAh Right Ascension (1975) h RAm Right Ascension (1975) min DE- Declination (1975) sign --- DEd Declination (1975) deg DEm Declination (1975) arcmin GLON Galactic longitude deg GLAT Galactic latitude deg Xpos Position eastwards on POSS blue print mm Ypos Position northwards on POSS blue print mm Mag Magnitude rounded to the nearest half magnitude mag r_Mag Source of Magnitude number=2 The magnitude sources are coded as follows: 1 de Vaucouleurs (RC1, 1964) 5 Collinder (1931) 2 Zwicky (1961-1968) <VII/49> 6 Arp (1965) <VII/13> 3 Vorontsov-Velyaminov <VII/62> 7 Vorontsov-Velyaminov (1931) 4 Lindsay =1958MNRAS.118..172L 8 Bok (1962), Van den Bergh (1968) The complete references are given in the file "adc.doc". --- OldDesc Visual appearance of object transcribed from Dreyer J.L.E. (1888( number=3 data blocks, separated by commas, each describing an aspect of the visual appearance of the object from Dreyer's (1888) catalogue. The appearance aspects are written in the following order: (a) For nebulae the sequence of blocks is: brightness, size, shape, radial brightness variation, comments referring to the field. (b) For clusters the sequence is: identification (cluster), size, richness, compression, brightness of the stars therein. The various codes and abbreviations are detailed in Table 5 of the file "adc.doc". --- NewDesc Palomar Sky Survey Description of each object number=4 The data blocks in the new description do not follow the regular sequence used in the old description. The description are decoded by taking each individual block of comma-separated data and finding the largest combination of letters present in the RNGC code table (Table 6 in file "adc.doc"). --- Notes Cross References for RNGC objects number=5 See Table 7 in file "adc.doc" for acronyms used in cross-references. --- adc.doc Documentation by Wayne H. Warren Jr. (1982) CDS 1995 Nov 04 UNKNOWN UNKNOWN * See Section 4 in file "adc.doc" * The catalogue was distributed on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1991), directory /nonstell/galaxies/rngc, as five files: the description (the present "adc.doc" file), the data file, old (Dreyer's) description supplement, new description supplement, and cross-reference supplements. * 15-Mar-1993: the four data files were merged into a single "catalog" file at CDS (Francois Ochsenbein). * 04-Nov-1995: this ReadMe file revisited at CDS. VII_1B.xml A Master List of Radio Sources 7002A VII/2A Master list of radio sources, updated 1978 A Master List of Radio Sources R S Dixon Astrophys. J. Suppl. Ser. 20 1 1970 1970ApJS...20....1D Radio sources The Master List of Radio Sources (MSL) has been prepared by combining about thirty catalogues in a common format. Approcimately 25000 listings are included for some 12000 separate sources.
The Master List Name Name of the object as assigned by the original author number=1 the used prefixes are detailed in file index. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Epoch ? yr Freq Frequency MHz l_S Limit flag on S: L = less than (<), G = greater than (>) --- S Flux density Jy RAorder "RA" for RA order list (always present) --- Version Version number (always 42) --- Seq Sequential order number --- Francois Ochsenbein CDS 1995 Sep 16 Bob Dixon, Ohio State University Radio Observatory <Bob_Dixon@osu.edu> UNKNOWN UNKNOWN * The tape was received at CDS from Dr Robert S. Dixon (Ohio State University Radio Observatory) in 1978; an explicit request of not distributing tape copies of the MSL existed until 1995. * 16-Sep-1995 (version 'A'): a few modifications was performed at CDS: => removed last (dummy) record => corrected shifted columns in records #36489, 49515, 52808, 78129 => Two unspecified values of the frequency exist in records #26475.58 and #40580.58 VII_2A.xml Catalogue of Abell and Zwicky Clusters of Galaxies 7004A VII/4A Abell and Zwicky Clusters of Galaxies Catalogue of Abell and Zwicky Clusters of Galaxies G O Abell Astrophys. J. Suppl. Ser. 3 211 1958 1958ApJS....3..211A Catalogue of Abell and Zwicky Clusters of Galaxies H G Corwin Jr. Astron. J. 79 1356 1974 1974AJ.....79.1356C Catalogue of Abell and Zwicky Clusters of Galaxies F Zwicky E Herzog P Wild M Karpowicz C T Kowal Catalogue of galaxies and of clusters of galaxies, California Institute of Technology, Pasadena, 6 vols. ??? ??? 1968 1968 Clusters, galaxy The catalog was originally prepared at the Bulgarian Academy of Sciences. The Abell clusters are rich, compact clusters of galaxies identified by Abell (1958). These clusters were identified on the red plates of the Palomar Observatory Sky Survey (POSS). The Zwicky clusters were identified by Zwicky et al. (1961-68) in 506 POSS fields. They are rich clusters, each having at least 50 members within 3 mag of the brightest member. The catalog includes cluster identification, several coordinate systems, magnitude of the tenth brightest cluster member, distance groups, richness groups, size, mean apparent population, and distance.
Abell Clusters (Abell, 1958; Corwin, 1974) Abell Abell cluster number --- n_Abell '2' if in Abell's statistical sample, '1' if not --- RAh Hours RA, 1950.0 h RAm Minutes RA, 1950.0 min DE- Sign Dec, 1950.0 --- DEd Degrees Dec, 1950.0 deg DEm Minutes Dec, 1950.0 arcmin Mag10 Magnitude of 10th brightest cluster member mag DistGroup Distance group number=1 DistGroup is Based on the magnitude of the 10th brightest member; it is defined as follows: '0'= < 13.3 '4'= 15.7 - 16.4 '1'= 13.3 - 14.0 '5'= 16.5 - 17.2 '2'= 14.1 - 14.8 '6'= 17.3 - 18.0 '3'= 14.9 - 15.6 '7'= > 18.0 --- RichGroup Richness group number=2 RichGroup depends on galaxy counts as follows: '0'= 30 - 40 '3'= 130 - 199 '1'= 50 - 79 '4'= 200 - 299 '2'= 80 - 129 '5'= 300 or over. --- GLON Galactic longitude deg GLAT Galactic latitude deg RLamb Lambert distance from pole number=3 The Lambert projection is an equal-area projection, where the distance to the center (nearest galactic pole) RLamb is defined by: RLamb = 2 sin (theta/2) where theta = polar distance = (90-b) and the position angle is the longitude. RLamb is negative for clusters located in southern galactic hemisphere. The Cartesian values XLamb and YLamb are defined by: XLamb = RLamb sin(l) (component directed toward l=90deg) YLamb = RLamb cos(l) (component directed toward l=0deg) RLamb, XLamb and YLamb are therefore in range [-sqrt(2), +sqrt(2)] --- XLamb Lambert X coordinate number=3 The Lambert projection is an equal-area projection, where the distance to the center (nearest galactic pole) RLamb is defined by: RLamb = 2 sin (theta/2) where theta = polar distance = (90-b) and the position angle is the longitude. RLamb is negative for clusters located in southern galactic hemisphere. The Cartesian values XLamb and YLamb are defined by: XLamb = RLamb sin(l) (component directed toward l=90deg) YLamb = RLamb cos(l) (component directed toward l=0deg) RLamb, XLamb and YLamb are therefore in range [-sqrt(2), +sqrt(2)] --- YLamb Lambert Y coordinate number=3 The Lambert projection is an equal-area projection, where the distance to the center (nearest galactic pole) RLamb is defined by: RLamb = 2 sin (theta/2) where theta = polar distance = (90-b) and the position angle is the longitude. RLamb is negative for clusters located in southern galactic hemisphere. The Cartesian values XLamb and YLamb are defined by: XLamb = RLamb sin(l) (component directed toward l=90deg) YLamb = RLamb cos(l) (component directed toward l=0deg) RLamb, XLamb and YLamb are therefore in range [-sqrt(2), +sqrt(2)] --- SGLON Supergalactic longitude (de Vaucouleur's system) deg SGLAT Supergalactic latitude deg ClusRad Corrected Abell cluster radius deg ClusArea Cluster area computed from ClusRad deg2 Pop Mean apparent population (galaxies/sq.deg) ct/deg2 Dist Radial distance to cluster Mpc DistX X component of Distance Mpc DistY Y component of Distance Mpc DistZ Z component of Distance Mpc Zwicky Clusters (Zwicky et al., 1961-68) Zwicky Zwicky cluster number --- RAh Hours RA, 1950.0 h RAm Minutes RA, 1950.0 min DE- Sign Dec, 1950.0 --- DEd Degrees Dec, 1950.0 deg DEm Minutes Dec, 1950.0 arcmin Type Cluster type number=1 Cluster type is '1'=open; '2'=medium compact; '3'=compact --- GalCnt Population of cluster (number of galaxies) --- Diam Diameter of cluster cm DistGroup Distance group number=2 DistGroup is: '1'= near '4'= very distant '2'= medium distant '5'= extremely distant '3'= distant --- GLON Galactic longitude deg GLAT Galactic latitude deg RLamb Lambert distance from pole number=3 Lambert projection is explained above in Note(3) of file: abell.dat. --- XLamb Lambert X coordinate number=3 Lambert projection is explained above in Note(3) of file: abell.dat. --- YLamb Lambert Y coordinate number=3 Lambert projection is explained above in Note(3) of file: abell.dat. --- SGLON Supergalactic longitude, de Vaucouleur's system deg SGLAT Supergalactic latitude deg ClusRad Cluster radius: 0.09326 * Diam deg ClusArea Cluster area: 0.02733 * Diam**2 deg2 Pop Mean apparent population (galaxies/sq.deg) ct/deg2 Zwicky Clusters index Zwicky Zwicky cluster number --- RAh Hours RA, 1950.0 h RAm Minutes RA, 1950.0 min DE- Sign Dec, 1950.0 --- DEd Degrees Dec, 1950.0 deg DEm Minutes Dec, 1950.0 arcmin Area1 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number1 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area2 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number2 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area3 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number3 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area4 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number4 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area5 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number5 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area6 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number6 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area7 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number7 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area8 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number8 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area9 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number9 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area10 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number10 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area11 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number11 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Area12 Plate area containing cluster number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- Number12 Cluster number within plate area number=1 Up to 12 Zwicky plate numbers and cluster numbers within the plates (a cluster often spreads into several plate areas). Pairs are sorted in order of increasing order of plate-area number. --- adc.doc Documentation written by Robert S. Hill Francois Ochsenbein CDS 1995 Apr 12 UNKNOWN UNKNOWN * The catalogue has been prepared initially by the Bulgarian Academy of Sciences * See in "adc.doc" file, section 4, from the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory: /cd6/nonstell/galaxies/abzwclus VII_4A.xml Excerpt from the Catalogue of Stars Clusters and Associations 7005A VII/5A Star Clusters and Associations, Selected Data Excerpt from the Catalogue of Stars Clusters and Associations G Alter J Ruprecht V Vanysek Akad. Kiado, Budapest, 3086 p., 2nd edition ??? ??? 1970 1970csca.book.....A VII/31B : Part I (Associations) VII/44B : Part II (Globular Clusters) VII/101 : Part III (Open Clusters) Alter, G., Balazs, B., and Ruprecht, J. 1970, Catalogue of Star Clusters and Associations, 2nd Edition, Akademiai Kiada Budapest, printed in Hungary (card form) Associations, stellar Clusters, open The catalog is a selection of data on all open clusters extracted from the second, considerably enlarged edition of the "Catalogue of Star Clusters and Associations" edited by Alter, Balazs, and Ruprecht (1970), which includes four parts: Part 1: 1039 open clusters, five moving clusters, and 11 stellar groups; Part 2: 70 OB associations; Part 3: 125 globular clusters; Part 4: 28 extragalactic objects. The catalog includes galactic and equatorial coordinates, name, classification, angular diameter, distance, magnitude and spectral types of the brightest stars, total magnitude, and color excess.
The Catalogue GLON Galactic longitude deg GLAT Galactic latitude deg RAh Hours RA, equinox 1950.0 h RAm Minutes RA, equinox 1950.0 min DE- Sign Dec, equinox 1950.0 --- DEd Degrees Dec, equinox 1950.0 deg DEm Minutes Dec, equinox 1950.0 arcmin Name Cluster name --- Class Trumpler class. codes, see below. The following coding is used: 32p = III 2 p 43pn = IV 3 p n, etc. --- Diam Angular diameter arcmin Dist Cluster distance pc Mag1 Magnitude of brightest stars in cluster mag SpType Spectral type --- Code1 Unidentified code --- IntMag Total or integrated magnitude of the cluster mag Code2 Unidentified code --- ColorEx Color excess of the cluster in UBV system mag Code3 Unidentified code --- CDS 1994 Mar 19 UNKNOWN UNKNOWN 1988 May: Wayne H. Warren Jr. Astronomical Data Center The machine-readable version of this compilation was received from the Centre de Donnees de Strasbourg in January 1979. A brief format description had been prepared there through a comparison of the data with the second edition of the published catalog, since the original description only consisted of the following statement: "The file contains information about coordinate type, distance, diameter, etc.... for all open clusters known in 1968." The original format was condensed and contained mostly integer numbers that were difficult to read and interpret. Therefore, the catalog format was modified and expanded at the Astronomical Data Center, NASA Goddard Space Flight Center, and this new description has been prepared for the new format. A copy of the original catalog was sent to Dr. Charles J. Peterson of the University of Missouri, Columbia, who prepared notes about the format and identification of many of the data, and the description below is based partly on these notes. We appreciate the efforts of Dr. Peterson in describing the data and returning this information to the ADC, and for communicating with us at length about the catalog. UNKNOWN UNKNOWN Trumpler classification system (see Trumpler, R. J. 1930, Lick Obs. Bull. 14, 154) First figure: Appearance (projected distribution of stars) I Detached cluster with strong central concentration. II Detached cluster with little central concentration. III Detached cluster with no noticeable concentration, i.e., a uniform distribution of stars within the cluster boundaries. IV Cluster that appears more like a star field concentration. Second figure: Stellar brightnesses 1 Most cluster stars are nearly of the same apparent brightness. 2 A medium range in the brightnesses of stars. 3 Bright and faint stars are both present. Generally a few very bright stars and some moderately bright stars embedded in a body of fainter stars can be seen. Third figure: Number of stars p a poor cluster, n < 50 stars. m a moderately rich cluster, 50 < n < 100 stars. r a rich cluster, n > 100 stars. Fourth figure: Other characteristics e elongated u asymmetrical n associated nebulosity VII_5A.xml Catalogue of Polarization Measurements and Related Data of Extragalactic Radio Sources 7006 VII/6 Polarization Meas Extragalactic Radio Sources Catalogue of Polarization Measurements and Related Data of Extragalactic Radio Sources W Eichendorf M Reinhardt Astrophysics and Space Science 61 153-167 1979 1979Ap&SS..61..153E Catalogue of Polarization Measurements and Related Data of Extragalactic Radio Sources W Eichendorf M Reinhardt Acta Cosmologica, Zesz. 9 7-48 1981 1981AcC.....9....7E Polarization Galaxies, radio Redshifts Galaxy catalogs The catalog contains 510 extragalactic radio sources, and covers all polarization measurements from 1965 to the middle of 1974 and a few other radio and optical data for these sources. The typical observation error was in the range of 1-2 percent in 1965 and 0.5-1 percent in 1974. The selection criterion for sources was that polarization data should be available at least at three wavelengths for each source. This reduced the sample to 510 sources. The catalog includes observational data: classifications, Cambridge numbers, coordinates, degrees of polarization at various wavelengths, polarization angles at each wavelength, largest angular diameters, position angles, and redshifts. The catalog also includes derived data: rotation measures, linear source diameters, polarization angles at wavelength 0 cm, differences between position angle and polarization angle at 0 cm, spectral indices between each pair of successive wavelengths observed, and polarization indices between each pair of successive wavelengths observed.
observed data 510 extragalactic radio sources RAh Right ascension in hours (B1950) Equatorial coordinates (1950.0) h RAm RA in minutes min DE- Sign of Declination --- DEd Declination in degrees (B1950) deg RC3REV Cambridge number Cambridge number. From the Revised 3C Catalog of Radio Sources (Bennett 1962). --- Class Classification One of three, single-letter classification codes: G = Radio Galaxy Q = Quasar U = Unidentified --- z Redshift --- AngDiam Largest angular diameter arcsec PA Position angle in degrees Position angle of the major axis of the object, measured eastward from North in degrees. deg S(2cm) Flux dens. at 2 cm Jy S(3.7cm) Flux dens. at 3.7 cm Jy S(6cm) Flux dens. at 6 cm Jy S(11cm) Flux dens. at 11 cm Jy S(18cm) Flux dens. at 18 cm Jy S(21cm) Flux dens. at 21 cm Jy S(31cm) Flux dens. at 31 cm Jy S(49cm) Flux dens. at 49 cm Jy S(73cm) Flux dens. at 73 cm Jy LP(2cm) Deg. of linear polarization 2 cm in percent % LP(3.7cm) Deg. of linear polarization 3.7 cm in perc % LP(6cm) Deg. of linear polarization 6 cm in percent % LP(11cm) Deg. of linear polarization 11 cm in perc % LP(18cm) Deg. of linear polarization 18 cm in perc % LP(21cm) Deg. of linear polarization 21 cm in perc % LP(31cm) Deg. of linear polarization 31 cm in perc % LP(49cm) Deg. of linear polarization 49 cm in perc % LP(73cm) Deg. of linear polarization 73 cm in perc % PolA(2cm) Pol. angle at 2 cm deg PolA(3.7cm) Pol. angle at 3.7 cm deg PolA(6cm) Pol. angle at 6 cm deg PolA(11cm) Pol. angle at 11 cm deg PolA(18cm) Pol. angle at 18 cm deg PolA(21cm) Pol. angle at 21 cm deg PolA(31cm) Pol. angle at 31 cm deg PolA(49cm) Pol. angle at 49 cm deg PolA(73cm) Pol. angle at 73 cm deg Derived values RAh Right ascension in hours (B1950) h RAm RA in minutes min DE- Sign of Declination --- DEd Declination in degrees (B1950) deg RC3REV Cambridge number --- Class Classification --- RM Rotation measure in radians per square meter rad/m2 PolA Pol. angle at 0 cm Linear extrapolation of the angle of polarization at wavelength = 0 cm, in degrees. deg PA-PolA Pos. angle - pol. angle Difference between the position angle of the source and the polarization angle at lambda = 0 cm in degrees. deg SI Mean spectral index The mean spectral index coefficient, found by regression, of the individual spectral indices. Note: All of these values were recalculated by the authors of the catalog even when accepted values already existed, because of the greater amount of data available to them. See Eichendorf and Reinhardt (1979) and Eichendorf and Reinhardt (1980) for discussions of how the recalculated mean spectral indices compare to the existing data. The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- PI Mean pol. index Analogous to the mean spectral index for flux densities, this is the coefficient found by regression from the individual polarization indices. The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- SI(2) Spec. index, 2-3.7 cm The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- SI(3.7) Spec. index, 3.7-6 cm The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- SI(6) Spec. index, 6 -11 cm The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- SI(11) Spec. index, 11-18 cm The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- SI(18) Spec. index, 18-21 cm The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- SI(21) Spec. index, 21-31 cm The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- SI(31) Spec. index, 31-49 cm The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- SI(49) Spec. index, 49-73 cm The spectral index SI(*) defined by a power law in the flux density function S, where S = frequency . power(SI(*)). Usually SI(*) is notated with the greek letter alpha. The spectral index is determined only between the available wavelengths. --- PI(2) Pol. index, 2-3.7 cm The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- PI(3.7) Pol. index, 3.7-6 cm The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- PI(6) Pol. index, 6 -11 cm The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- PI(11) Pol. index, 11-18 cm The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- PI(18) Pol. index, 18-21 cm The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- PI(21) Pol. index, 21-31 cm The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- PI(31) Pol. index, 31-49 cm The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- PI(49) Pol. index, 49-73 cm The polarization index PI(*) is defined as a power law analogous to the spectral index for the flux density measurements. The degree of polarization, P = frequency. power(PI(*)). As in the case of the spectral index, PI(*) is defined only between certain wavelengths. This quantity was introduced and defined by the authors and included in the catalog. See both references for details of the derivation, justification, and implications of this parameter. --- Redshift-corrected data RAh Right ascension in hours (B1950) h RAm RA in minutes min DE- Sign of Declination --- DEd Declination in degrees (B1950) deg RC3REV Cambridge number --- Class Classification --- LP(2cm) Deg. of linear polarization 2 cm in percent % LP(3.7cm) Deg. of lin. polarization 3.7 cm in percent % LP(6cm) Deg. of linear polarization 6 cm in percent % LP(11cm) Deg. of linear polarization 11 cm in percent % LP(18cm) Deg. of linear polarization 18 cm in percent % LP(21cm) Deg. of linear polarization 21 cm in percent % LP(31cm) Deg. of linear polarization 31 cm in percent % LP(49cm) Deg. of linear polarization 49 cm in percent % LP(73cm) Deg. of linear polarization 73 cm in percent % PolA(2cm) Pol. angle at 2 cm deg PolA(3.7cm) Pol. angle at 3.7 cm deg PolA(6cm) Pol. angle at 6 cm deg PolA(11cm) Pol. angle at 11 cm deg PolA(18cm) Pol. angle at 18 cm deg PolA(21cm) Pol. angle at 21 cm deg PolA(31cm) Pol. angle at 31 cm deg PolA(49cm) Pol. angle at 49 cm deg PolA(73cm) Pol. angle at 73 cm deg S(2cm) Flux dens. at 2 cm Jy S(3.7cm) Flux dens. at 3.7 cm Jy S(6cm) Flux dens. at 6 cm Jy S(11cm) Flux dens. at 11 cm Jy S(18cm) Flux dens. at 18 cm Jy S(21cm) Flux dens. at 21 cm Jy S(31cm) Flux dens. at 31 cm Jy S(49cm) Flux dens. at 49 cm Jy S(73cm) Flux dens. at 73 cm Jy Redshift-corrected derived values RAh Right ascension in hours (B1950) h RAm RA in minutes min DE- Sign of Declination --- DEd Declination in degrees (B1950) deg RC3REV Cambridge number --- Class Classification --- Diam Lin. source diam. Line source diameter. In Mpc. See Eichendorf and Reinhardt (1980) for details of how this was derived. Mpc RM Rotation measure in radians per square meter Rotation measure. Derived from the redshift-corrected values, in radians per square meter. rad/m2 PolA Pol. angle at 0 cm deg PA-PolA Pos. angle - pol. angle deg SI Mean spectral index --- PI Mean pol. index --- SI(2) Spec. index, 2-3.7 cm --- SI(3.7) Spec. index, 3.7-6 cm --- SI(6) Spec. index, 6 -11 cm --- SI(11) Spec. index, 11-18 cm --- SI(18) Spec. index, 18-21 cm --- SI(21) Spec. index, 21-31 cm --- SI(31) Spec. index, 31-49 cm --- SI(49) Spec. index, 49-73 cm --- PI(2) Pol. index, 2-3.7 cm --- PI(3.7) Pol. index, 3.7-6 cm --- PI(6) Pol. index, 6 -11 cm --- PI(11) Pol. index, 11-18 cm --- PI(18) Pol. index, 18-21 cm --- PI(21) Pol. index, 21-31 cm --- PI(31) Pol. index, 31-49 cm --- PI(49) Pol. index, 49-73 cm --- C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 05 The original ADC documentation by Theresa A. Nagy (1979) was used to generate this ReadMe file. UNKNOWN UNKNOWN The Catalog of Polarization Measurements and Related Data of Extragalactic Radio Sources was sent to the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, by the Centre de Donnees Astronomiques, Strasbourg (CDS), in July 1980. The original tape contained four text files formatted in the same manner as in the published catalog. The catalog was so well formatted that essentially no editing was required. VII_6.xml Catalogue of Dark Nebulae 7007A VII/7A Lynds' Catalogue of Dark Nebulae Catalogue of Dark Nebulae B T Lynds Astrophys. J. Suppl. Ser. 7 1 1962 1962ApJS....7....1L VII/191 : Catalogue of Southern Dark Clouds (Hartley+ 1986) J/A+AS/113/325 : Distance measurements of some Lynds nebulae (Hilton+ 1995) Nebulae This catalog is an updated version from the published version. The catalog was based on the red and blue prints of the National Geographic - Palomar Observatory Sky Atlas. The catalog contains positions, both equatorial and galactic for the centers of dark nebulae. Values for the cloud sizes are given in square degrees, and estimates of their opacity are given. The updated catalog is ordered by galactic longitude and includes cross references to the published catalog and Barnard Object numbers associated with the clouds.
The LDN Catalogue LDN Catalogue number from original published version (ApJS 7, 1) Compared to the printed edition: => 15 "duplicated" LDN numbers were removed: 184, 366, 457, 465, 924, 1025, 1318, 1342, 1344, 1413, 1575, 1592, 1593, 1603, 1792 => there are 4 nebulae without a LDN number at the end of the table --- RAh Right Ascension 1950 (hours) of Cloud Center h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) of Cloud Center --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin GLON Galactic longitude of Cloud Center deg GLAT Galactic latitude of Cloud Center deg Area Area, in square degrees, of the Cloud deg2 Opacity Opacity class The opacity is on a scale of 1 (lightest) to 6 (darkest). in cases where small dark clouds are within large, lighter clouds, both or all clouds have been listed separately. But they will be identified with the same ID (bytes 48-50) number. --- ID Identification Number. Entries with null identification number are objects lying in the general obscuration of the Milky Way. --- Seq Running Number in this version of the Catalogue (ordered by GLON) --- Lynds2 Number that B. Lynds assigned when the updated catalogue was created. Number that B. Lynds assigned when the updated catalogue was created. The significance of this number is unknown. Also, it is not a unique number throughout this version of the catalogue. --- Barn Cross-identifications with Barnard Objects. (up to 8 Barnard numbers in format 8A4) Barnard designations are made by a number followed by a letter; see Barnard E.E., 1927, Carnegie Inst. Washington, "A photographic Atlas of selected regions of the Milky Way" --- James Marcout, Francois Ochsenbein CDS 1996 Feb 22 UNKNOWN UNKNOWN * July 1979, by Theresa A. Nagy, from NASA document R-SAW-7/79-13, "Documentation for the machine-readable version of Lynds' Catalogue of Dark Nebula": The initial version of the machine-readable version of the Lynds' Catalogue of Dark Nebulae was received from the University of Maryland. This version was obtained from the author and represents an updated version of the original published catalogue (1962 Astrophysical Journal Supplement #64). The major differences between these two versions are as follows: 1. The galactic coordinates have been revised. 2. Some of the original observations of "clouds" have been deleted. 3. There are 1791 objects in the updated version and there were 1802 objects in the original published catalogue. The original version, as such, does not exist in machine-readable form except in the cases where we have added the Barnard identification(s) to the appropriate objects. Since a correlation had to be made from the original catalogue numbers to obtain the Barnard cross-identifications (data obtained from a table in the original publication), these original numbers were retained. The version of the catalogue as received from the University of Maryland was updated as follows: 1. The catalogue was sorted by galactic longitude. 2. A running number (Seq) was added after the sort. 3. A cross-reference table between the old Lynds numbers and the Barnard numbers was made so that this information could be added to the machine-readable version. Therefore, the Barnard numbers and the original Lynds numbers were added (one record had as many as eight Barnard numbers). * October 1991: the catalogue is prepared for the ADC CD-ROM "Selected Astronomical Catalogs" Vol. 1 (NASA), in directory /nonstell/nebulae/ldn * 25-Sep-1995: Description added by Gail L. Schneider [SSDOO/ADC] * 22-Feb-1996: James Marcout and Francois Ochsenbein, CDS) The previous version only contained a fraction of LDN numbers (about 1500 were missing). A new version 'A' of the catalogue was created, incorporating all original LDN numbers, with the exception of nebulae originally duplicated (see Note on LDN above); the columns were re-ordered to follow more closely the original publication. VII_7A.xml Catalogue of bright nebulae 7009 VII/9 Lynds' Catalogue of Bright Nebulae Catalogue of bright nebulae B T Lynds Astrophys. J. Suppl. Ser. 12 163 1965 1965ApJS...12..163L Nebulae H II regions The Catalogue of Bright Nebulae lists the galactic and equatorial coordinates of the center of the cloud, the dimensions of the nebulae as measured on the photograph on which it appeared at its brightest, the area of nebulosity in square degrees, color as compared between the blue and red Palomar plates, a brightness index on a scale of 6, an identification number that indicates the complexity of the nebulosity, and a cross reference to NGC (Cat. <VII.1>), Index Catalogue (IC), Sharpless (1959) Catalogue of HII Regions (Cat. <VII/20>), Cederblad (1956) Catalogue of Diffuse Galactic Nebulae, and Dorschner and Gurtler (1963).
The LBN Catalogue Seq Running number number=1 This number represents the sequence in the published paper; see also the History below. --- GLON Galactic longitude of cloud center deg GLAT Galactic longitude of the cloud center deg RAh Hours RA, 1950.0 h RAm Minutes RA, 1950.0 min DE- Sign Dec, 1950.0 --- DEd Degrees Dec, 1950.0 deg DEm Minutes Dec, 1950.0 arcmin Diam1 Largest dimension of nebula arcmin Diam2 Smallest dimension of nebula arcmin Area Area of nebulosity deg2 Color Color index number=2 The following codes are used for Color: '1' if brighter on blue Palomar plate; '2' if equal on red and blue Palomar plates; '3' if brighter on red Palomar plate; '4' if visible only on the red Palomar plate. This parameter is zero only for the two nebulae #191 (074.53-08.42 = NGC 6960) and #844 (189.13+02.97 = IC 443) --- Bright Brightness scale number=3 the brightness scale varies from '1' (brightest) to '6' (barely detectable). This parameter is zero only for the sane two nebulae #191 (074.53-08.42 = NGC 6960) and #844 (189.13+02.97 = IC 443) --- ID Identification number number=4 ID indicates whether or not the object is an isolated region (=0) or a region of different brightness located in a more extensive complex of nebulosities. --- Name Other name of nebulosity number=5 Abbreviations are NGC = New General Catalogue (NGC, cat. <VII/1>) IC = Index Catalogue S = Sharpless HII Regions (Sh 2-), 1959, Cat. <VII/20> C = Catalogue of Diffuse Galactic Nebulae, Cederblad 1959, Medd. Lund Ser.2, No 119 DG = Dorschner and Gurtler 1963, AN 287, 257 --- Francois Ochsenbein CDS 1996 Dec 16 UNKNOWN UNKNOWN * The catalogue is extracted (in June 1994) from the CD-ROM of NASA/ADC "Selected Astronomical Catalogs Vol. 1" with the following corrections: - #582 (118.25+04.84) (shifted column) - Nebulae with identical central positions where checked against the publication and reordered according to the published catalogue. The following galactic central positions refer to 2 or more nebulae: 007.03-02.26 008.44+36.18 011.54+36.11 014.12+00.06 020.36-01.27 021.10-00.60 078.21+02.48 084.28-01.32 084.81+03.88 085.58+04.24 112.16+00.23 118.25+04.84 123.88-01.93 166.39-23.63 169.24-00.94 184.36-28.85 189.78-13.76 194.69-15.60 204.44-00.56 204.60-13.66 206.39-01.87 206.90-16.56 208.69-02.51 243.16+00.32 353.76+17.61 * The first "Seq" column, a number which is now found in the literature, was added at CDS in December 1996. VII_9.xml Share Quasar Catalog, Selected Data including the Kitt Peak Quasar Catalog Sources. 7011 VII/11 Share Quasar Cat, Selected Data Share Quasar Catalog, Selected Data including the Kitt Peak Quasar Catalog Sources. G Share Private Communication, ca. ??? ??? 1975 1975 QSOs This catalog includes the complete source list with positions of the Kitt Peak Quasar Catalog (de Veny et al., 1971). Other fields in the de Veny catalog (4C ID, B1950 equatorial positions, V, B-V, U-B, z, references to ID UBV z, and Notes and other references) are not included. The Kitt Peak Quasar Catalog sources were selected based on optical data for all confirmed quasars published prior to May or June 1971. This includes objects with only one spectral line. The published catalog includes a bibliography for all quasars with redshifts The source list also includes some additional sources included by the author.
Quasar ID and positions ID Name of celestial object --- RAdeg Right Ascension in degrees (1950.0) deg DEdeg Declination in degrees (1950.0) deg Flag data Source (1=de Veny et al.; 2=unknown) --- N.P.M. Kuin & C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 04 The original ADC documentation by Theresa A. Nagy (1979) was used to generate this ReadMe file. Kuin verified the sources and added the flag column. UNKNOWN UNKNOWN The De Veny Kitt Peak Quasar Catalogue (J. B. De Veny, W. H. Osborn and K. Janes 1971, Publications of the Astronomical Society of the Pacific, 83, 611) source list with position has been made machine-readable by Dr. G. Share (Naval Research Laboratory). The information given in this document has been obtained via private communication from Dr. Share. No effort has been expended to verify the contents and Dr. Share bears the responsibility for any keypunching errors. The original data file had a column marked X-ray data with zero values throughout and a blank notes field. These were removed for the current update. The data were checked against the publication list of source names and a flag for the original de Veny et al. sources was added. The origin of the other sources is from Share. VII_11.xml Globular-Cluster Catalog 7013 VII/13 Globular-Cluster Catalog Globular-Cluster Catalog H C Arp Stars and Stellar Systems, Vol. 5, gen. ed. G.P. Kuiper, eds. A. Blaauw and M . Schmidt, Chapter 19, p. 410. ??? ??? 1965 1965 Clusters, globular This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.
*Catalog Data ID NGC number or other 102 clobular clusters have NGC designations 2 are listed in the Index catalogues --- n_ID note Unmarked entries of Spectral Type are from Kron and Mayal (1960) : uncertain value 1 from V(hor br), table 6 in reference 2 adjusted to RR Lyrae distance scale via figure 7 in reference 3 Spectral type from Kinman (1959b). 4 Kinman (1959b) gives F2 5 Arp-Van den Bergh 6 Kinman (1959b) gives F3 --- name cluster name --- Con_Cl Concentration Class The roman numerals have been replaced by arabic numerals. --- u_Con_Cl uncertainty indicator Concentration Class --- RAh Right Ascension hours (1950.0) h RAm Right Ascension minutes (1950.0) min DE- Declination sign (1950) --- DEd Declination degrees (1950) deg DEm Declination arc minutes (1950) arcmin GLON Galactic Longitude l II deg n_GLON note to GLON --- GLAT Galactic Lattitude b II deg ABS_LAW Galactic Absorption from formula 0.24 csc b --- A(B) Kron-Mayal case II absorption law mag D(0.9) Diameter (containing 0.9 of the light) arcsec u_D(0.9) uncertainty indicator Diameter --- Bmean Mean B mag of 25 brightest stars The apparent B magnitudes of the mean of the 25 brightest stars. Older photographic magnitudes have all been corrected using the photometric recalibration of the Selected Areas and the color index correction to the B system by Arp. Bmean can be used to estimate the distance of the cluster based on a mean intrinsic magnitude M(B) = -0.8 mag. This is used to derive the Dmod value. mag Dmod distance modulus (m-M)app from Bmean --- n_Dmod note to Dmod --- r galactic radius from Dmod and ABS_LAW, Fig.7 kpc x Sun centered galactic X-coordinate The coordinate system x,y, and z is centered on the Sun, with x directed toward the galaxy center, y in the direction of the rotation, and z perpendicular to the plane. In order to get a coordinate sytem with its center at the center of the galaxy it is only neccesary to substract Ro, the distance between the Sun and the center of the galaxy, from x. Other parameters: Cluster mass. Only for 2 clusters the mass was determined based on the intermal kinematics. These are M92 (110,000 Msun) and 47 Tuc (2.5 to 6 million Msun). kpc y galactic y-coordinate in direction rotation kpc z height above galactic plane kpc Btot apparent integrated B brightness Apparent magnitudes measured by kron and Mayal (1960) were transformed into the Johnson V system, transformed color indices were applied to derive Btot. Absolute magnitudes M(B) were found for the clusters that have distances using the csc reddening law. Earlier measures of integrated globular cluster magnitudes by Christie (Hogg 1959) can be compared to the Kron-Mayal measures. Transforming both measures to the B system, it can be shown that they correlate well. The data for 12 additional clusters based on the Christie measures were included. mag B-V apparent color from Kron and Mayal (1960) mag M(B) absolute magnitudes from Btot mag (B-V)o intrinsic color using E(B-V) = 0.06 csc b mag Sp spectral type from Kron and Mayal (1960) --- n_Sp note on Spectral type --- RV cluster radial velocity km/s N.P.M. Kuin ADC 1996 Apr 24 UNKNOWN UNKNOWN Arp's Globular Cluster Catalogue has been made machine-readable by Dr. N.P.M. Kuin at the ADC since catalog was requested frequently and the original version submitted by Dr. G. Share only contained ID and positions. VII_13.xml Galactic Supernova Remnants Catalogue 7014 VII/14 Galactic Supernova Remnants Catalogue Galactic Supernova Remnants Catalogue D H Clark J L Caswell Mon. Not. Roy. Astron. Soc. 174 267 1976 1976MNRAS.174..267C Supernova remnants Radio sources The catalog contains observations for southern galactic supernova remnants (SNRs). The observations were made at 408 MHz with the one-mile cross-type radio telescope at the Molonglo radio observatory between 1969 December and 1971 June and were made at 5000 MHz with the Parkes 64-m radio telescope between 1968 May and 1973 April. The catalog has two files (two tables in published version). The first file lists the 97 known SNRs south of declination +18 degrees (i.e., within the scope of the Molonglo survey and gives Molonglo and Parkes observational data where available). For completeness the 23 known SNRs north of declination +18 degrees are listed in a second file. The catalog includes identifications, the 408-MHz integrated flux densities, mean angular diameters, and surface brightnesses of the SNRs.
Southern (Dec < +18 deg) galactic SNRs ID Galactic source number --- Alt Other catalogue number or name --- n_S(408) Flux density flag 1 "(" If flux densities are estimates as obtained by Shaver and Goss from fitting Gaussians to the individual source brightness distributions (1970 Aust. J. Phys. Astrophys. Suppl. No. 14, 133). ")" Same as above. "*" estimated flux density is not obtained from the Molonglo pencil-beam survey. --- S(408) Integrated flux density estimate at 408 MHz Jy n_S(408)b Flux density flag 2 --- n_S(5000) Flux density flag 3 --- S(5000) Integrated flux density at 5000 MHz Jy n_S(5000)b Flux density flag 4 --- n_SI Spectral Index flag 1 "(" If data other than at 408 and 5000 MHz were used to compute the spectral index between 408 and 5000 MHz. ")" Same as above. --- SI Spectral index between 408 and 5000 MHz Spectral index for those sources with flux density estimates available at the two frequencies. --- n_SIb Spectral Index flag 2 "(" If data other than at 408 and 5000 MHz were used to compute the spectral index between 408 and 5000 MHz. ")" Same as above. --- l_AngDiam " < " or " > " where applicable "<" or ">" mean less or larger than the size of the angular diameter of remnant. --- AngDiam Angular diameter of remnant (arc minutes) arcmin B(408) Surface brightness at 408 MHz W/m2/sr/Hz r_S(408) Original reference to 408 MHz flux density "revised" implies a reassessment of the earlier Molonglo data by the authors. --- r_S(5000) Original reference to 5000 MHz flux density --- MapRef Map reference (where possible Molonglo maps) --- Southern (Dec > +18 deg) galactic SNRs ID Galactic source number --- Alt Other catalogue number or name --- n_S(408) Flux density flag 1 See Notes given for data1.dat --- S(408) Integrated flux density estimate at 408 MHz Jy n_S(408)b Flux density flag 2 --- n_S(5000) Flux density flag 3 --- S(5000) Integrated flux density at 5000 MHz Jy n_S(5000)b Flux density flag 4 --- n_SI Spectral Index flag 1 --- SI Spectral index between 408 and 5000 MHz --- n_SIb Spectral Index flag 2 --- l_AngDiam " < " or " > " where applicable --- AngDiam Angular diameter of remnant (arc minutes) arcmin B(408) Surface brightness at 408 MHz W/m2/sr/Hz RefList List of references to recent data List of references to recent observational data for each source --- r_SI Reference for spectral index information --- MapRef Map reference of the source Map reference of the source with brightest resolution available --- Sv Spectral Index defined by S(alpha)v(alpha) Spectral Index defined by S(alpha)v(alpha) between 408 and 5000 MHz for those sources with flux density estimates available at the two frequencies. The definition of alpha, nor v is given here. --- C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 08 The original ADC documentation by Theresa A. Nagy (1979) was used to generate this ReadMe file. UNKNOWN UNKNOWN This galactic supernova remnant catalogue was made machine-readable at the Goddard Space Flight Center. The data is from the paper "A study of Galactic Supernova Remnants, Based on Molonglo-Parkes Observational Data" by D. H. Clark and J. L. Caswell (Mon. Not. Royal Astronomical Society, 1976, 174, 267-305). The two data files represent the data from sources south of declination +18 degrees and sources north of declination +18 degrees, respectively. VII_14.xml Galactic Supernova Remnants Catalogue 7015 VII/15 Galactic Supernova Remnants Catalogue Galactic Supernova Remnants Catalogue S A Ilovaisky J Lequeux Astron. & Astrophys. 18 169 1972 1972A&A....18..169I Supernova remnants Radio sources Radio-frequency absorption line observations of 20 sources were used to calibrate the relation between radio surface brightness and linear diameter. Distances for 116 SNR were derived using the new calibration. The catalog lists galactic longitude and latitude in decimal degrees, source name, flux density (in 10-26 W m-2 Hz-1) at 1 GHz, mean angular diameter of the source (arcmin), surface brightness at 1 GHz, diameter of the remnant (pc), distance of the remnant (kpc), scale height from the galactic plane (pc), radial distance to the center (kpc), and references (by number given in the original publication).
Galactic SNRs Catalog Data GLON Galactic longitude l(II) deg GLAT Galactic latitude b(II) deg flag "*" if not a supernova remnant "*" if the source is not a supernova remnant (SNR) according to Clark and Caswell list. --- ID Name of source --- S Flux density at one gigahertz in flux units 1 flux unit = 10-26 W m-2 Hz-1 Jy AngDiam Mean angular diameter of source arcmin B Surface brightness at one gigahertz W/m2/sr/Hz Diam Diameter of the remnant in parsecs pc D Distance of the remnant kpc H Scale height from galactic plane pc RadGCen Radial distance from the galactic center kpc Ref References --- C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 08 The original ADC documentation by Theresa A. Nagy (1979) was used to generate this ReadMe file. VII_15.xml Reference Catalogue of Bright Galaxies 7016 VII/16 Reference Catalogue of Bright Galaxies Reference Catalogue of Bright Galaxies G de Vaucouleurs A de Vaucouleurs The Reference Catalogue of Bright Galaxies, Univ. of Texas Press, Austin ??? ??? 1964 1964rcbg.book.....D Galaxies Active gal. nuclei Bibliography Catalogs The Reference Catalogue of Bright Galaxies lists for each entry the following information: NGC number, IC number, or A number; A, B, or C designation; B1950.0 positions, position at 100 year precession; galactic and supergalactic positions; revised morphological type and source; type and color class in Yerkes list 1 and 2; Hubble-Sandage type; revised Hubble type according to Holmberg; logarithm of mean major diameter (log D) and ratio of major to minor diameter (log R) and their weights; logarithm of major diameter; sources of the diameters; David Dunlap Observatory type and luminosity class; Harvard photographic apparent magnitude; weight of V, B-V(0), U-B(0); integrated magnitude B(0) and its weight in the B system; mean surface brightness in magnitude per square minute of arc and sources for the B magnitude; mean B surface brightness derived from corrected Harvard magnitude; the integrated color index in the standard B-V system; "intrinsic" color index; sources of B-V and/or U-B; integrated color in the standard U-B system; observed radial velocity in km/sec; radial velocity corrected for solar motion in km/sec; sources of radial velocities; solar motion correction; and direct photographic source. The catalog was created by concatenating four files side by side.
Bright Galaxies Reference Data cat1 catalog identification catalog identification coded as NGC#, IC#, or A# ("N", "I", or "A" respectively). --- ID1 Catalog number 1 --- suffix1 A, B, or C designation --- RAh Right ascension, hours (1950.0) h RAm Right ascension, minutes (1950.0) min DEd Declination (1950.0) degrees deg DEm Declination, arc minutes (1950.0) arcmin GLON1 Galactic longitude (l(I), degrees) deg GLON2 Galactic longitude (l(II), degrees) deg SGLON Supergalactic longitude (degrees) deg RMtype Revised morphological type and source --- TC_Yerk1 Type and color class in Yerkes list 1 --- HStype Hubble-Sandage type --- log(D) Logarithm of mean major diameter 0.1arcmin log(R) Log of mean ratio of major diameter to minor --- log(MaD) Logarithm of major diameter in units of 0'.1 0.1arcmin Source1 Sources of log(D) and log(R) --- line The number 2 indicates start of second line --- cat2 NGC#, IC#, or A# NGC#, IC#, or A# (repeat data, see bytes 2-6) --- ID2 Catalog number 2 --- flag2 A, B, or C designation --- PRAh+100 Precession in RA(hours) for 100 yrsn h/ha PRAm+100 Precession in RA(minutes) for 100 years min/ha PDEd+100 Precession in DEC(deg) for 100 years deg/ha PDEm+100 precession in DEC(arcmin) for 100 yrs arcmin/ha GLAT1 Galactic latitude (b(I), degrees) deg GLAT2 Galactic latitude (b(II), degrees) deg SGLAT Supergalactic latitude (degrees) deg TypLumCl Type and luminosity class David Dunlap Observatory type and luminosity class --- TC_Yerk2 Type and color class in Yerkes list 2 --- RHubType Revised Hubble type according to Holmberg --- w_log(D) Weight of log(D) --- w_log(R) Weight of log(R) --- Source2 Sources of log(D) and log(R) continued --- cat3 NGC#, IC#, or A# --- ID3 Catalog number 3 --- flag3 A, B, or C designation (repeat data) --- HphotoM Harvard photographic apparent magnitude mag note "*" See the notes in the original reference --- B(0) Integrated magnitude in the B system B(0). mag BsurfBr1 Mean B surface brightness mag/arcmin2 Source3 Sources of B magnitude --- B-V(0) Integrated color index in the B-V system --- u_B-V(0) '*' means uncertain values in B-V --- IntrinCI Intrinsic color index. --- Source4 Sources of B-V or U-B Sources of B-V and data after the symbol / is the source of U-B --- U-B(0) Integrated color index in the U-B system --- u_U-B(0) '*' means uncertain values in U-B --- RV Observed radial velocity km/s RVC Radial velocity corrected for solar motion km/s Source5 Sources of radial velocities --- Cflux Radio (continuum) flux Radio (continuum) flux at some standard wavelength integrated flux in the 21-cm HI emission line; both fields are currently blank. --- Source6 Direct photographic source --- cat4 NGC#, IC#, or A# --- ID4 Catalog number 4 --- flag6 A, B, or C designation (repeat data) --- HphotoMC Harvard photographic magnitude corrected Harvard photographic magnitude statistically corrected mag w_B(0) Weight of B(0) (cf. bytes 172-176) --- BsurfBr2 Mean B surface brightness Mean B surface brightness derived from corrected Harvard magnitude --- Source7 Sources of B magnitude (continued) --- w_B-V(0) Weight of B-V(0) (cf. bytes 187-192) --- Source8 Sources of B-V and U-B colors continued --- w_U-B(0) Weight of U-B(0) (cf bytes 202-206) --- w_RV Weight of Radial Velocity --- SolarC Solar motion correction km/s source9 Sources of RV (continued from bytes 217-221) --- unknown unexplained extra characters --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Nov 08 The original ADC documentation by Theresa A. Nagy (1979) was used to generate this ReadMe file. UNKNOWN UNKNOWN The machine-readable version of the de Vaucouleurs' Galaxy catalogue was received through a copy at the University of Pennsylvania (March 1975). The last tape record was incomplete and this was corrected by using the information from the hard copy version of the catalogue. Initially, the tape version had four records for each entry of the catalogue. The first two records corresponded to the two lines of data on the left-hand page of the hard copy. The third and fourth records corresponded to the two lines of data per entry on the right-hand page of the hard copy version of the catalogue. Each of these records were initially 138 bytes in length and it was determined that only the first 80 bytes of each record contained catalogue data and that the remaining part of the record was blank. The catalogue was then run through a short program which concatenated the first 80 bytes of each of the four records and output one record, 320 bytes in length, per entry in the catalogue. VII_16.xml Catalogue of HII Regions 7020 VII/20 Catalogue of HII Regions Catalogue of HII Regions S Sharpless Astrophys. J. Suppl. Ser. 4 257 1959 1959ApJS....4..257S H II regions Nebulae The catalogue describes the position, maximum angular diameters, classifications according to form, structure and brightness, and the number of associated stars. The acronym used in the literature to designate objects from this catalogue is Sh 2 (e.g. Sh 2-1 for the first HII region of the catalogue)
The Sharpless (Sh 2) Catalogue Sh2 Sharpless HII catalog number --- GlLund Galactic longitude based on Lund pole 0.1deg GbLund Galactic latitude based on Lund pole 0.1deg GLon Galactic longitude number=1 Not in the original publication 0.1deg GLat Galactic latitude number=1 Not in the original publication 0.1deg RAh1900 Hours RA, 1900.0 h RAm1900 Minutes RA, 1900.0 min RAds1900 Deci-seconds RA, 1900.0 0.1s DE-1900 Sign Dec, 1900.0 --- DEd1900 Degrees Dec, 1900.0 deg DEm1900 Minutes Dec, 1900.0 arcmin DEs1900 Seconds Dec, 1900.0 arcsec RAh Right Ascension (hours) 1950 number=1 Not in the original publication h RAm Right Ascension (minutes) 1950 number=1 Not in the original publication min RAds Right Ascension (deci-seconds) 1950 number=1 Not in the original publication 0.1s DE- Declination (sign) 1950 number=1 Not in the original publication --- DEd Declination (degrees) 1950 number=1 Not in the original publication deg DEm Declination (minutes) 1950 number=1 Not in the original publication arcmin DEs Declination (seconds) 1950 number=1 Not in the original publication arcsec Diam Maximum angular diameter of H II region arcmin Form Classification as to form: 1=circular; 2=elliptical; 3=irregular --- Struct Classification as to structure, from 1=amorphous to 3=filamentary --- Bright Classification as to brightness, from 1=faintest to 3=brightest --- Stars Number of associated stars with the H II region --- adc.doc ADC Documentation by Theresa A. Nagy Francois Ochsenbein CDS 1995 Jan 31 UNKNOWN UNKNOWN * 31-Jan-1995: From the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory /nonstell/nebulae/hii with a few modifications: => The 'S' in column 1 has been dropped => The blank hours of RA 1900 were transformed to zero. VII_20.xml Catalogue of Reflection Nebulae 7021 VII/21 Catalogue of Reflection Nebulae Catalogue of Reflection Nebulae S Van den Bergh Astron. J. 71 990 1966 1966AJ.....71..990V Nebulae A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.
The catalogue (Table I of publication) VdB van den Bergh catalog number number=1 a 159th reflection nebula corresponding to HD 224403 (GLON=116.6, GLAT=-00.22) is introduced by R. Racine in his study of stars in Reflection Nebulae in (1968AJ.....73..233R) --- RemFlag '*' if remark is given in the publication --- DM Durchmusterung (BD, CD or CP) designation --- HD Henry Draper Catalog (HD) number --- HD2 HD number suffix if second designation given --- GLON Galactic longitude deg GLAT Galactic latitude deg SpType Spectral type --- Vmag V magnitude mag n_Vmag 'V' if variable magnitude --- Type Type of nebula, see Note number=2 Types given are I, II, I-II, II P, II, or P. P is peculiar, and Type I and II are defined as follows: Type I: nebula in which the illuminating star is embedded in the nebulosity; Type II: star located outside the illuminated nebulosity. --- SurfBr Surface brightness on the blue PSS prints number=3 Brightness is coded as: 'VBR'=very bright; 'BR'=bright; 'M'=moderate; 'F'=faint; 'VF'=very faint; ':'=uncertain. --- Color Coded reference to colors, see Note number=4 Color classes are coded as: 'VB'=very blue; 'B'=blue; 'MB'=moderately blue; 'I'=intermediate 'MR'=moderately red; 'R'=red; 'VR'=very red; ':'=uncertain. --- Absorb Absorption in field of nebula number=5 Absorption is noted as: 'STR'=strong; 'MOD'=moderate; 'WK'=weak; 'ABS'=absent --- BRadMax Maximum radii observed on blue PSS prints arcmin u_BRadMax Uncertainty flag (:) on BRadMax --- RRadMax Maximum radii observed on red PSS prints arcmin u_RRadMax Uncertainty flag (:) on BRadMax --- Francois Ochsenbein CDS 1995 Aug 23 UNKNOWN UNKNOWN * NASA/ADC: The machine-readable version of the van den Bergh Reflection Nebulae Catalogue was received from the University of Maryland. The original card deck was in the 026 punch and this was converted to a 029 deck. Two keypunch errors were corrected in the 029 version: #34 - the spectral type was changed from 09.5V to O9.5V (zero to oh) #112 - the brightness was changed from ";"to "F" * July 1979: documentation of the electronic version prepared by Theresa A. Nagy (Document R-SAW-7/79-04 at NASA-GSFC, Greenbelt) * Prepared in directory /nonstell/nebulae/reflect of CD-ROM "Selected Astronomical Catalogs Volume 1" edited by the Astronomical Data Center, NASA, 1992. * 23-Aug-1995: Inserted missing decimal points in radius columns, and added this standardized documentation file (at CDS) * 28-Apr-1998: NASA/ADC corrected spectral type and visual magnitude entries for 104. VII_21.xml A Catalogue of Absorption Lines in QSO Spectra 7023 VII/23 Absorption Lines in QSO Spectra A Catalogue of Absorption Lines in QSO Spectra R S Ellis S Phillipps Mon. Not. Roy. Astr. Soc. 183 271 1978 1978MNRAS.183..271E QSOs Spectroscopy The catalog is a collection of spectral data for 128 quasi-stellar objects (QSO). The data have been assembled from the catalogs of de Veny et al. (1971), Smith-Haenni (1977), and Burbidge et al. (1977). To ensure every observation is recorded and to search for new or omitted results, the entire literature up to 1977 September was scanned. The catalog distributed by the ADC is an updated version of the original catalog published as microfiche in Ellis and Phillipps (1978). The catalog includes object names, positions and identifications, V, B-V, U-B, emission redshifts, observation references, analyses, and line lists. The lists of observed spectral lines come from many observers and instruments. References to observations and to analyses are included for each QSO, as are alternate names for the QSO, coordinates, and magnitude. Each observed line has a reference to the observer, and most have the possible line identifications and redshifts listed as well. See the original paper for a discussion of the purpose behind the compilation of the catalog, in particular, for a discussion of its use as a base of raw spectral data that is not tied to any particular redshift system.
Identification of each object ID Object running number --- Ident Object identifiers Ellis and Phillipps adopted the coordinate notation of Burbidge, Crowne, and Smith (1977; BCS) as their primary identifier (bytes 5-14). Alternate names are listed in rough order of occurrence in the literature (bytes 15-76). --- LineRec Number of line data records The total number of line data records for this QSO. --- Coordinates ID Object running number --- RAtag Right Ascension tag, "RA=" --- RAh RA hours (B1950) h RAm RA minutes min RAs RA seconds s Dectag Declination tag, "DEC=" --- DE- Dec sign --- DEd Dec degrees (B1950) deg DEm Dec arc minutes arcmin DEs Dec arc seconds arcsec IDtag ID reference tag The character string "FC:" if the ID reference has a finding chart; or the character string "ID:" if the ID reference gives only an identification. --- IDref ID reference Reference to the identification of the QSO. --- Magnitudes ID Object running number --- Magtag Magnitude tag, "V=" --- Vmag Visual magnitude The visual magnitude and colors come almost exclusively from BCS and range from pure estimates to accurate photometry. If no data are available, the character string "-0." appears in this field and in the color fields. mag Varflag Variability flag An asterisk, "*", indicates variability; a question mark, "?", indicates doubt about the magnitude. --- B-Vtag B-V color tag, "B-V=" --- B-V B-V color mag U-Btab U-B color tag, "U-B=" --- U-B U-B color mag Ztag Emission redshift tag, "ZEM=" --- Z Emission redshift Other published values for the redshift are given in the notes. --- q_Z Redshift quality flag A question mark, "?", denotes uncertainty in the redshift other than that due to a low number of observed lines. Generally, the uncertainty is due to a wide spread from line to line. --- Lflag Left parenthesis --- Nline Number of emission lines Number of permitted emission lines with the quoted emission redshift. This number is enclosed by parentheses in bytes 43 and 46. --- Rflag Right parenthesis --- line data ID Object running number --- Lstflag Last line flag The character "+" if this is the last spectral line for which data are given, otherwise blank. There may be one or more continuation records, however, before the next group begins; see the description of observed wavelength below. --- ObsWave Observed wavelength The observed wavelength, in angstroms, given to the quoted accuracy. If this field is blank, the identified ion, ion rest wavelength, actual redshift, and system numbers are a continuation of the previous record. 0.1nm Gsymbol Group symbols Various characters such as "#", "%", "&", etc. used by Ellis and Phillipps to associate "different wavelengths reported by different observers that clearly relate to a single spectral line. According to Ellis' and Phillipps' opinion all wavelengths sharing the same symbol belong to one line. --- RefNum Observer reference number The observer reference number as given in the observation group or the analysis group. --- S-EW Strength or equivalent width Strength or equivalent width. The relative strength of the line is given on an increasing scale of 1 to 5 (0 means the strength was not given). A "+5" indicates unusually strong lines, "-1" indicates unusually weak lines, and a preceding "=" indicates joint strength lines. Relative widths and equivalent widths to the nearest angstrom (in the observer's frame) are given when available. The following notation is used to qualify the strengths: B - blend T - trough W - equivalent width in angstroms ? - questionable E - emission - - shortward in wavelength + - longward in wavelength For example, BE- says the absorption line is blended into the blue side of an emission line. In some cases, the observer ref. # field overflows into this field, indicating that more than one observer has reported the observed wavelength. A comma, ",", will appear in byte 17 when this happens, and byte 18 will have the reference number of the second observer. --- Ion Identified ion The element and level of ionization identified with the observed wavelength. --- RestWave Ion rest wavelength 0.1nm Z Actual redshift When high-precision results are given, the redshifts were calculated using vacuum wavelengths. --- SysNum System numbers These numbers refer back to the system numbers described below. See the description of the analyses and system records for obs.dat. --- notes ID Object running number --- note General notes for each object --- C.-H. Joseph Lyu Hughes STX/NASA 1996 May 10 The original ADC documentation by Lee E. Brotzman (1986) was used to create this ReadMe file. UNKNOWN UNKNOWN The Catalogue of Absorption Lines in QSO Spectra was sent to the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, by the Centre de Donnees Stellaires (CDS), in July 1980. This version consisted of two files: the original file used to produce the microfiche for Ellis and Phillipps (1978), and an updated version in the same format. Only the updated file is being distributed by the ADC; it is, therefore, the one described in this document. Some checking and reformatting were done by the ADC, although no data values were altered. (However, some bibliographical information was corrected.) Fortran programs were written to separate the "groups" of records for each QSO, and the groups were proofread and checked for format consistency. Errors and format problems were corrected with a text editor. Other programs were written to check the formats more closely. The index file was produced by ADC personnel. The original reformatted Catalogue of Absorption Lines in QSO Spectra thus consisted of two files: the catalog file itself (data.dat) and an index file (index.dat). The catalog file had multiple records for each object, and the records were not identically formatted. The index file had a single record for each object, and the records were identically formatted. The records for each object are assembled into the following groups: names, coordinates, magnitudes, observations/analyses, line data and notes. The formats for each group are different, and two groups -- the analyses and notes -- may not even be present at all. Because of the complications in the non-identical and multiple formats of the records of each object, specifically in those of the groups of observations, analyses, and systems (i.e., in obs.dat, see below), we have to separate out obs.dat from the original catalog file and put the identically formatted groups in our new ADC catalog files, id.dat, mag.dat, lines.dat, and note.dat, respectively. Brief Description of obs.dat: As explained above, we don't have a unique byte-by-byte description for obs.dat. However, the researcher should be able to obtain complete information based upon the object running number. For some QSO objects, there may be either no observational data or no analysis and system group records. The general formats for the groups of observations, analyses, and systems are given as follows. Bytes Format Units Label Explanations 1-3 I3 --- ID Object running number 7-18 A12 --- Obstag Observations tag, "OBSERVATIONS" 1-3 I3 --- ID Object running number 7-8 A2 --- RefNum Reference number 10-45 A36 --- Ref Complete Reference for the observed lines 47-56 A10 0.1nm Wave Wavelength region covered by the observations 58-64 A5 --- Restag Resolution tag, "RESN" or "RADIO" 63-68 F6.2 0.1nm Res Resolution in the units of the cited paper 69-72 A4 --- Disptag Dispersion tag, "DISP" 73-79 F7.2 0.1nm/mm Disp Dispersion in the units of the cited paper 80 A1 --- q_Disp Dispersion quality, "?" means uncertained value 1-3 I3 --- ID Object running number 7-14 A8 --- Anatag Analyses tag, "ANALYSES" The records in the analysis group fall into two categories: analysis records and system records. Ellis and Phillips define a redshift system as "a collection of two or more lines ... having approximately the same" absorption redshift. An analysis is an article reporting one or more systems. Each object may have a number of analysis records. Each analysis is represented by one analysis record followed by a set of 1 to 45 system records. Occasionally, the system records are followed by one or more records containing notes. The note record can be identified by a sharp or pound sign (#) in byte 7. The remaining bytes contain the text of the note. The analysis record gives a reference to the paper and information on the number of absorption lines and systems. The system records give more specific data about each system. For the reference, if the reference number is the same as that of a record in the observation group, the reference has only the author and year of publication; otherwise, a full reference is given. 1-3 I3 --- ID Object running number 7-8 A2 --- RefNum Reference number 10-45 A36 --- Ref Reference 46-49 I4 --- Numline Number of absorption lines (from the paper) 51-54 A4 --- Linetag Lines tag, "LINES" 56-59 I4 --- Nident Number of identifications (from the paper) 61-65 A5 --- Identtag Identifications tag, "IDENT" 66-68 I3 --- NumSys Number of redshift systems (from the paper) 70-76 A7 --- Systag Systems tag, "SYSTEMS" or "SYSTEM " 1-3 I3 --- ID Object running number 7 A1 --- Notetag Note flag, "#" means a note about the analysis 26-30 A5 --- SysNum System number, e.g., 3.02 refers to the second system in analysis paper 3 31-38 F8.5 --- Avg-Z The mean absorption redshift of the system to the accuracy quoted 39-41 I3 --- Nline Number of lines making up the redshift system 43-47 A4 --- Linetag Lines tag, "LINES" 50-54 F5.2 0.1nm WaveErr Mean wavelength error for the observer's frame of reference 55 A1 --- Wavetag Wavelength tag, "A", only in the 1st system record of each analysis 59 A1 --- Lparen Left parenthesis 60 I1 --- R-Est Reality estimate 61 A1 --- Rparen Right parenthesis The reality estimate is a relative estimate of the reality of the system on the following scale: 3 = certain 2 = probable 1 = possible 0 = not given The reality estimate is enclosed by left and right parentheses in bytes 59 and 61, respectively. VII_23.xml Uppsala General Catalogue of Galaxies (UGC) 7026D VII/26D Uppsala General Catalogue of Galaxies Uppsala General Catalogue of Galaxies (UGC) P Nilson Uppsala Astron. Obs. Ann. 6 ??? ??? 1973 1973ugcg.book.....N Galaxy catalogs The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalogue of galaxies to a limiting diameter of 1.0' and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5degrees. Galaxies smaller than 1.0' in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are ordered by 1950 right ascension. The catalogue contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version. The order of the records is strictly by UGC number; i.e., the Addenda records follow their main catalogue counterparts in the file. The colons (indicating uncertainty) and various other codes (parentheses, brackets) are not included in the machine-readable version of the catalogue. Several possible improvements to the catalogue might consist of adding codes corresponding to the published version, a second file containing abbreviations and terminology and a third file with the extensive notes. It would also be important to add an asterisk or some other code to data records having a note in the proposed third file. This document describes the machine-readable version of the UGC as distributed by the Astronomical Data Centers. It is intended to enable users to read and process the data without problems or guesswork. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted. A copy of this document should accompany any machine-readable copy of the catalogue.
UGC catalogue UGCtext "UGC" --- UGC UGC number --- A "A" if the galaxy is from the Addenda list of the published catalogue; otherwise blank. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin MCG MCG designation number=1 The Morphological Catalogue of Galaxies (MCG) <Catalogue: VII/62A> (Vorontsov-Velyaminov et al. 1962, 1963, 1964, 1968). The first number of the designation is the Palomar Observatory Sky Survey (POSS) 6deg zone, from the equator +00 to the north celestial pole +15; the second number is the POSS field along the zone, while the third number is the galaxy in this field in the MCG. Non-MCG galaxies are assigned the number 000 in the third position, but the first and second values are given correctly. --- POSS Number of the POSS field in which the galaxy is best visible. --- MajAxis Major axis of the galaxy as measured on the POSS blue print. number=2 The precision to which diameters are recorded matches the published catalogue; additional decimal places are blank, but colons, brackets and parentheses are not included in the computerized catalogue. arcmin MinAxis Minor axis of the galaxy as measured on the POSS blue print. number=2 The precision to which diameters are recorded matches the published catalogue; additional decimal places are blank, but colons, brackets and parentheses are not included in the computerized catalogue. arcmin PA Position angle measured in the conventional manner from North through East. number=3 Colons, parentheses and brackets in the published catalogue are not included here. Blank if data not present. deg Hubble Classification in the Hubble system or remarks, in a free field format, including lower case designations. --- Pmag Photographic magnitude mpg , recorded to precision given in published catalogue; i.e., if tenths not reported, byte 64 is blank. mag RadVel Radial velocity corrected for Solar motion number=4 Radial Velocity is relative to the Local Group according to V0 = 300 cos A, where A is the distance to the conventional Solar apex at lI=55deg, bI=0deg or lII = 87deg bII = +1deg. If the uncertainties in the measurements were considered too large to make corrections meaningful, usually only the uncorrected value is given. km/s aR Major axis of the galaxy as measured on the POSS red print. number=2 The precision to which diameters are recorded matches the published catalogue; additional decimal places are blank, but colons, brackets and parentheses are not included in the computerized catalogue. arcmin bR Minor axis of the galaxy as measured on the POSS red print. number=2 The precision to which diameters are recorded matches the published catalogue; additional decimal places are blank, but colons, brackets and parentheses are not included in the computerized catalogue. arcmin i Inclination to the line of sight for spirals number=5 Inclination measured on a scale from 1 (face-on) to 7 (edge-on). For galaxies of high inclination, a value is calculated from the Hubble formula n - 10(a-b)/a [a - major axis, b - minor axis]. The value 7 denotes objects inclined not more than a few degrees to the line of sight. --- The changes made by the ADC in 1995 ID Number of entry --- IDs Suffix for entry number --- field Field in error --- old Old entry --- new New entry and comments --- Nancy Grace Roman ADC/SSDOO 1995 Oct 20 The present version includes a few corrections inserted by CDS (see Remarks, Modifications, points 8 and 9) compared to the CD-ROM "Selected Astronomical Catalogs Volume 1" edited by the Astronomical Data Center, NASA, 1992. It also contains a number of corrections inserted by the undersigned. The latter are listed in errors.dat. Points 8 and 9, the "File Summary" and the "Byte-by-byte Description" were prepared by Francois Ochsenbein of the CDS. The file errors.dat and minor modifications to this acknowledgment were prepared by the undersigned. Otherwise, the documentation herein is from Wayne H. Warren Jr. (1982). The latter expressed appreciation to Dr. R. S. Dixon for supplying the original tape version of the UGC, and to Mr. M. Schmitz for pointing out the errors that he discovered in the UGC numbers (point 3 above). Nancy G. Roman expresses appreciation particularly to Mark Anderson who did an extensive analysis of the catalog. Others errors were reported by Ralph Pass, Carlo Giovanardi, and James Himer. All have been checked and most reported errors were correct as reported. UNKNOWN UNKNOWN The magnetic tape version of the Uppsala General Catalogue of Galaxies was received from Dr. Robert S. Dixon of the Ohio State University Radio Observatory on 7 December 1981. As received, the catalogue consisted of 12,942 logical records of length 90 bytes. Each logical record contained a sequential counter on bytes 85-90, while bytes 81-84 and single columns throughout the records were not used. There was also only a five-byte allowance for the major axis of the galaxy as measured on the red POSS print, a field too small to accommodate U00454 (M31), which has a major axis of 200:' (in order to fit the 200' value, the radial velocity had been moved left one byte, thus making it read -2990 km/sec instead of the correct value of -299 km/sec). The following modifications were made to the catalogue to fix the above items, correct several errors, and to maximize storage efficiency. Except for item 10, these modifications were made by Francois Ochsenbein at the CDS. 1.The published edition contains 12,921 objects in the main catalogue and 19 addenda; hence, with 12,942 records on the tape there were obviously a few duplicates. The records for UGC 3944 and UGC 6063A were found to be repeated and the duplicates were deleted. 2.A check for the addenda objects resulted in the discovery of a missing A for UGC 7399A--this was added. 3.Upon examination of the original file version of the catalogue supplied to him, Mr. Marion Schmitz discovered the misnumbering of UGC 12417 and UGC 12418 as UGC 12447 and UGC 12448--these errors were corrected. 4.The data record for UGC 253 was found to have a hexadecimal code "AA" character (equivalent to a down-arrow in the classification field (bytes 46-52) in place of a lower case "b" (Sb/SB(down-arrow) instead of Sb/SBb)--this was corrected. 5.The data field for the major axis as measured on the red POSS print was expanded to six bytes and the record for UGC 454 (discussed above) corrected. 6.All superfluous blanks were removed to decrease the logical record length from 90 bytes to 74 bytes (counting also the removal of the sequential numbers originally in bytes 85-90). 7.UGC and MCG catalog designations were altered to their present format, extending the record length to 81 bytes. 8.(Version C, made at CDS, August 1993) a. The error reported by Carlo Giovanardi in "ADC Newsletter" 2.2 (April 1993) was corrected (RAh column) b. The position of the minor axis blue in UGC 326 which was shifted has been fixed. c. All records with radial velocities larger than 10000 km/s expanded over the red major axis column; the + sign in column 65 was therefore removed for the following galaxies: UGC 262 UGC 545 UGC 1095 UGC 4093 UGC 5408 UGC 6514 UGC 8058 UGC 8327 UGC 8696 UGC 8811 UGC 8825 UGC 9509 UGC 10099 UGC 10170 UGC 10180 UGC 10188 UGC 10189 UGC 10191 UGC 10192 UGC 10199 UGC 10635 UGC 11130 UGC 11763 UGC 12397 d. UGC Number 20016 should be read 12016 Position angles for UGC 153, 341 and 388 were corrected (S. Nishimura, on 30-Aug-1993) 9.(Version D, made at CDS September 1995, following comments by Ralph Pass <rppass@tasc.com>), typo errors in UGC numbers: 4500 5228 5258 7307 10374 10377 10848 11718 11748 12342 12392 12847 12848 12817 12818 12843 12873 10.At least one error may have been corrected inappropriately. UGC5206 and 5854A are both given as MGC+02-28-002 but UGC 5206 is at RA=0941.7 while the MGC galaxy is at RA=1041.7. 5854A is at that location. It was assumed that these referred to the same galaxy. Hence UGC5854A was deleted and the RA changed for UGC5206 by the undersigned. She also moved two records which were out of order to the proper position. VII_26D.xml Catalogue of Star Clusters and Associations, Supplement 1, Associations 7031B VII/31B Star Clusters/Associations. I. Associations Catalogue of Star Clusters and Associations, Supplement 1, Associations J Ruprecht B Balazs R E White Akademiai Kiado, Publ. House Hungarian Acad. Sciences, Budapest ??? ??? 1981 1981 Catalogue of Star Clusters and Associations, Supplement 1, Associations J Ruprecht B Balazs R E White Bull. Inform. CDS 22 132 1982 1982BICDS..22..132R VII/5 : Excerpt of the Catalogue (catalogue) VII/44 : Part II (Globular clusters, catalogue) VII/101 : Part III (Open Clusters, catalogue) Alter, G., Balazs, B., and Ruprecht, J., 1970, Catalogue of Stellar Clusters and Associations, 2nd edition, Akademiai Kiada, Budapest, printed in Hungary Ruprecht, J., Balazs, B. and White, R.E., 1982, Catalog of Star Clusters and Associations, Supplement 1, Vols. I-III, Bull. Inform. CDS, no. 22, p. 132 Bibliography Associations, stellar The catalog contains data and bibliographical citations for all 70 associations of the second edition of the "Catalogue of Star Clusters and Associations (CSCA)" edited by Alter et al. (1970) which includes data for open clusters, associations, globular clusters and extragalactic objects up to 1967 and "Supplement to the CSCA" by Ruprecht et al. (1982), which contains the supplementary data up to the end of 1973. Thus, the literature is covered through 1973. The catalog includes the years of the literature, references, authors, abbreviated journal references, diameters, distances and color indices of the associations, number of stars and spectral types of the stars in the associations, and identification of the Palomar Observatory Sky Survey Chart on which the association appears.
List of associations and their positions Assoc Association number starting with ASS --- Page Card (or page) number of the second edition (missing for ASS-3) --- Name Other name of the association --- GLON Galactic longitude number=1 the position was added at CDS for additional associations, i.e. ASS names with decimal figures. These positions have generally less accuracy. Note also that the last association ASS-70 has no position: it lays over tens of degrees. deg GLAT Galactic latitude number=1 the position was added at CDS for additional associations, i.e. ASS names with decimal figures. These positions have generally less accuracy. Note also that the last association ASS-70 has no position: it lays over tens of degrees. deg RAh Right Ascension 1950 (hours) number=1 the position was added at CDS for additional associations, i.e. ASS names with decimal figures. These positions have generally less accuracy. Note also that the last association ASS-70 has no position: it lays over tens of degrees. h RAm Right Ascension 1950 (minutes) number=1 the position was added at CDS for additional associations, i.e. ASS names with decimal figures. These positions have generally less accuracy. Note also that the last association ASS-70 has no position: it lays over tens of degrees. min DE- Declination 1950 (sign) number=1 the position was added at CDS for additional associations, i.e. ASS names with decimal figures. These positions have generally less accuracy. Note also that the last association ASS-70 has no position: it lays over tens of degrees. --- DEd Declination 1950 (degrees) number=1 the position was added at CDS for additional associations, i.e. ASS names with decimal figures. These positions have generally less accuracy. Note also that the last association ASS-70 has no position: it lays over tens of degrees. deg DEm Declination 1950 (minutes) number=1 the position was added at CDS for additional associations, i.e. ASS names with decimal figures. These positions have generally less accuracy. Note also that the last association ASS-70 has no position: it lays over tens of degrees. arcmin POSS Palomar Sky Survey chart with its RA and Dec --- X Position on the chart from lower left corner mm Y Position on the chart from lower left corner mm Designations of each association Num Association number --- m_Num Association number suffix (e.g. .1 for 50.1) --- Desig List of association designations used by various authors --- Page Card (or page) number of the second edition (missing for ASS-3) --- Bibliography with parameters by reference Num Association number number= (1) = DIE ENTSTEHUNG VON STERNEN,SPRINGER,BERLIN (2) = ATLAS OF COL-MG DIAGR.,SUPPLEMENT,MOSCOW (3) = PR.UN.PB.S2,N37-40,32 (4) = PR.UN.PB,S2,N37-40,34 (5) = CAN.J.R.A.S,46,222 (6) = WIEN.AN,29,N3 (PUP I,II) number= The aggregated data and notes combined into the the Misc column do not follow a strict column structure. For many records, the notes start at the beginning of this field (byte 52). Other records contain some or all of the following subfields loosly adhering to the byte ranges shown: 52- 55 DIST: Distance of the association (pc) 57- 60 LD: Linear diameter of the association (pc) 65- 67 N: Number of stars in the association 69- 74 MG: Type of photometric magnitudes 76- 81 CI: Color index of the association 83- 87 SP: Spectra 88- 92 P: Positions 94-141 NOTE: Notes --- m_Num Association number suffix (e.g. .1 for 50.1) number= (1) = DIE ENTSTEHUNG VON STERNEN,SPRINGER,BERLIN (2) = ATLAS OF COL-MG DIAGR.,SUPPLEMENT,MOSCOW (3) = PR.UN.PB.S2,N37-40,32 (4) = PR.UN.PB,S2,N37-40,34 (5) = CAN.J.R.A.S,46,222 (6) = WIEN.AN,29,N3 (PUP I,II) number= The aggregated data and notes combined into the the Misc column do not follow a strict column structure. For many records, the notes start at the beginning of this field (byte 52). Other records contain some or all of the following subfields loosly adhering to the byte ranges shown: 52- 55 DIST: Distance of the association (pc) 57- 60 LD: Linear diameter of the association (pc) 65- 67 N: Number of stars in the association 69- 74 MG: Type of photometric magnitudes 76- 81 CI: Color index of the association 83- 87 SP: Spectra 88- 92 P: Positions 94-141 NOTE: Notes --- Year Year of the literature reference number= (1) = DIE ENTSTEHUNG VON STERNEN,SPRINGER,BERLIN (2) = ATLAS OF COL-MG DIAGR.,SUPPLEMENT,MOSCOW (3) = PR.UN.PB.S2,N37-40,32 (4) = PR.UN.PB,S2,N37-40,34 (5) = CAN.J.R.A.S,46,222 (6) = WIEN.AN,29,N3 (PUP I,II) number= The aggregated data and notes combined into the the Misc column do not follow a strict column structure. For many records, the notes start at the beginning of this field (byte 52). Other records contain some or all of the following subfields loosly adhering to the byte ranges shown: 52- 55 DIST: Distance of the association (pc) 57- 60 LD: Linear diameter of the association (pc) 65- 67 N: Number of stars in the association 69- 74 MG: Type of photometric magnitudes 76- 81 CI: Color index of the association 83- 87 SP: Spectra 88- 92 P: Positions 94-141 NOTE: Notes yr Author Author Name number= (1) = DIE ENTSTEHUNG VON STERNEN,SPRINGER,BERLIN (2) = ATLAS OF COL-MG DIAGR.,SUPPLEMENT,MOSCOW (3) = PR.UN.PB.S2,N37-40,32 (4) = PR.UN.PB,S2,N37-40,34 (5) = CAN.J.R.A.S,46,222 (6) = WIEN.AN,29,N3 (PUP I,II) number= The aggregated data and notes combined into the the Misc column do not follow a strict column structure. For many records, the notes start at the beginning of this field (byte 52). Other records contain some or all of the following subfields loosly adhering to the byte ranges shown: 52- 55 DIST: Distance of the association (pc) 57- 60 LD: Linear diameter of the association (pc) 65- 67 N: Number of stars in the association 69- 74 MG: Type of photometric magnitudes 76- 81 CI: Color index of the association 83- 87 SP: Spectra 88- 92 P: Positions 94-141 NOTE: Notes --- ref Literature reference (1) = DIE ENTSTEHUNG VON STERNEN,SPRINGER,BERLIN (2) = ATLAS OF COL-MG DIAGR.,SUPPLEMENT,MOSCOW (3) = PR.UN.PB.S2,N37-40,32 (4) = PR.UN.PB,S2,N37-40,34 (5) = CAN.J.R.A.S,46,222 (6) = WIEN.AN,29,N3 (PUP I,II) number= (1) = DIE ENTSTEHUNG VON STERNEN,SPRINGER,BERLIN (2) = ATLAS OF COL-MG DIAGR.,SUPPLEMENT,MOSCOW (3) = PR.UN.PB.S2,N37-40,32 (4) = PR.UN.PB,S2,N37-40,34 (5) = CAN.J.R.A.S,46,222 (6) = WIEN.AN,29,N3 (PUP I,II) number= The aggregated data and notes combined into the the Misc column do not follow a strict column structure. For many records, the notes start at the beginning of this field (byte 52). Other records contain some or all of the following subfields loosly adhering to the byte ranges shown: 52- 55 DIST: Distance of the association (pc) 57- 60 LD: Linear diameter of the association (pc) 65- 67 N: Number of stars in the association 69- 74 MG: Type of photometric magnitudes 76- 81 CI: Color index of the association 83- 87 SP: Spectra 88- 92 P: Positions 94-141 NOTE: Notes --- AD Apparent diameter of the association number= (1) = DIE ENTSTEHUNG VON STERNEN,SPRINGER,BERLIN (2) = ATLAS OF COL-MG DIAGR.,SUPPLEMENT,MOSCOW (3) = PR.UN.PB.S2,N37-40,32 (4) = PR.UN.PB,S2,N37-40,34 (5) = CAN.J.R.A.S,46,222 (6) = WIEN.AN,29,N3 (PUP I,II) number= The aggregated data and notes combined into the the Misc column do not follow a strict column structure. For many records, the notes start at the beginning of this field (byte 52). Other records contain some or all of the following subfields loosly adhering to the byte ranges shown: 52- 55 DIST: Distance of the association (pc) 57- 60 LD: Linear diameter of the association (pc) 65- 67 N: Number of stars in the association 69- 74 MG: Type of photometric magnitudes 76- 81 CI: Color index of the association 83- 87 SP: Spectra 88- 92 P: Positions 94-141 NOTE: Notes arcmin Misc Aggregated data and notes The aggregated data and notes combined into the the Misc column do not follow a strict column structure. For many records, the notes start at the beginning of this field (byte 52). Other records contain some or all of the following subfields loosly adhering to the byte ranges shown: 52- 55 DIST: Distance of the association (pc) 57- 60 LD: Linear diameter of the association (pc) 65- 67 N: Number of stars in the association 69- 74 MG: Type of photometric magnitudes 76- 81 CI: Color index of the association 83- 87 SP: Spectra 88- 92 P: Positions 94-141 NOTE: Notes number= (1) = DIE ENTSTEHUNG VON STERNEN,SPRINGER,BERLIN (2) = ATLAS OF COL-MG DIAGR.,SUPPLEMENT,MOSCOW (3) = PR.UN.PB.S2,N37-40,32 (4) = PR.UN.PB,S2,N37-40,34 (5) = CAN.J.R.A.S,46,222 (6) = WIEN.AN,29,N3 (PUP I,II) number= The aggregated data and notes combined into the the Misc column do not follow a strict column structure. For many records, the notes start at the beginning of this field (byte 52). Other records contain some or all of the following subfields loosly adhering to the byte ranges shown: 52- 55 DIST: Distance of the association (pc) 57- 60 LD: Linear diameter of the association (pc) 65- 67 N: Number of stars in the association 69- 74 MG: Type of photometric magnitudes 76- 81 CI: Color index of the association 83- 87 SP: Spectra 88- 92 P: Positions 94-141 NOTE: Notes --- James E. Gass SSDOO/ADC 1998 Feb 13 UNKNOWN UNKNOWN The original catalog contained multiple record formats in one file. The file "names.dat" has been created from the first record per association. The file "assoc.dat" has been created from second records; missing positions were filled with approximative values found in the literature. The file "refs.dat" was created from the third and following records for each association. VII_31B.xml The ESO/Uppsala Survey of the ESO(B) Atlas 7034C VII/34C ESO/Uppsala Survey of the ESO The ESO/Uppsala Survey of the ESO(B) Atlas A Lauberts European Southern Observatory ??? ??? 1982 1982ESO...C......0L VII/115 : Surface Photometry of the ESO-Uppsala Galaxies (Lauberts+ 1989) Lauberts, A. 1984, private communication. Holmberg, E. B., Lauberts, A., Schuster, H. -E., West, R. M. 1974, A. & A. Suppl., 18, 463. (1974A&AS...18..463H) Holmberg, E. B., Lauberts, A., Schuster, H. -E., West, R. M. 1974, A. & A. Suppl., 18, 491. (1974A&AS...18..491H) Holmberg, E. B., Lauberts, A., Schuster, H. -E., West, R. M. 1975, A. & A. Suppl., 22, 327. (1975A&AS...22..327H) Holmberg, E. B., Lauberts, A., Schuster, H. -E., West, R. M. 1977, A. & A. Suppl., 27, 295. (1977A&AS...27..295H) Holmberg, E. B., Lauberts, A., Schuster, H. -E., West, R. M. 1978, A. & A. Suppl., 31, 15. (1978A&AS...31...15H) Holmberg, E. B., Lauberts, A., Schuster, H. -E., West, R. M. 1978, A. & A. Suppl., 34, 285. (1978A&AS...34..285H) Holmberg, E. B., Lauberts, A., Schuster, H. -E., West, R. M. 1980, A. & A. Suppl., 39, 173. (1980A&AS...39..173H) Lauberts, A., Holmberg, E. B., Schuster, H. -E., West, R. M. 1981, A. & A. Suppl., 43, 307. (1981A&AS...43..307L) Lauberts, A., Holmberg, E. B., Schuster, H. -E., West, R. M. 1981, A. & A. Suppl., 46, 311. (1981A&AS...46..311L) "Reference Catalog of Bright Galaxies", de Vaucouleurs, G., de Vaucouleurs, A. 1964, University of Texas Press, Austin. "The Second Reference Catalog of Bright Galaxies", de Vaucouleurs, G., de Vaucouleurs, A., Corwin, H. G. 1976, University of Texas Press, Austin. (Cat. <VII/112>) "The Morphological Catalog of Galaxies" (MCG), Vorontsov-Velyaminov, B. A. and Ahripova, A. A. 1968, Moscow: Sternberg Institute 38. (See cat. <VII/62> and <VII/100>) "Atlas and catalog of Interacting Galaxies" Vorontsov-Velyaminov, B.A., Sternberg Inst., Moscow, 1959 "Atlas and Catalog of Peculiar Galaxies", Arp, H. 1966, California Institute of Technology, Pasadena. (see cat. <VII/74>) "Catalog of Star Clusters and Associations", Alter, G., Balazs, B., and Ruprecht, J. 1970, 2nd edition, Budapest. (see cat. <VII/44>) Surveys Nonstellar objects Atlases Galaxy catalogs The survey is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1-m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2-mm GG385 filter were used to give a passband similar to the Johnson B color. The actual search was conducted at the Uppsala Observatory and resulted in a list of nonstellar objects including all NGC and IC galaxies between -20 and -30 degrees declination, all galaxies down to a limiting diameter of 1.0 arcmin, all disturbed galaxies as faint as possible, all star clusters in the Catalog of Star Clusters and Associations (Alter et al. 1970) and smaller and fainter clusters if recognizable and all planetary nebulae listed in the available catalogs. The catalog includes coordinates, identifications, diameters, position angles, morphological types, classifications, magnitudes, colors, and radial velocities.
The Catalogue RAh Hours RA, equinox 1950 h RAm Minutes RA, equinox 1950 min RAs Seconds RA, equinox 1950 s DE- Sign Dec, equinox 1950 --- DEd Degrees Dec, equinox 1950 deg DEm Minutes Dec, equinox 1950 arcmin ESO ESO/Uppsala descriptive identifier number=1 ESO designation is written FFF-oooNNN, where FFF = Field (plate) number, see file "plates.dat" ooo = Object class with * = star ** = double or multiple star SC = star cluster N = nebula A = asteroid C = comet G = galaxy IG = interacting galaxy EN = emission nebula PN = planetary nebula RN = reflection nebula SNR = supernova remnant ? = questionable object NNN = number within field --- ID Other identifier number=2 Some common abbreviations include: N for NGC, I for IC, M for Messier, PK for Perek-Kohoutek planetary nebulae, and GCl or OCl for star clusters from the Budapest catalog. References to these and other abbreviations are detailed in file "idrefs.dat" --- GLON Galactic longitude deg GLAT Galactic latitude deg X X plate coordinate (positive toward East) mm Y Y plate coordinate (positive toward North) mm MajAxis Major axis diameter 0.1arcmin u_MajAxis ':' if major axis is uncertain --- MinAxis Minor axis diameter 0.1arcmin u_MinAxis ':' if minor axis is uncertain --- PA Position angle of major axis from north through east deg u_PA ':' if position angle is uncertain --- MType Morphological type in RC2 system (de Vaucouleurs et al., 1976) --- Class Estimated Hubble class --- Desc Description --- FlagN '*' if note exists in file "notes.dat" --- FlagM '1' if galaxy listed in MCG --- FlagRC '2' if galaxy listed in RC2 --- FlagV 'V' if galaxy listed in Vorontsov-Velyaminov (1959) --- FlagA 'A' if galaxy listed in Arp (1966) --- Bmag B magnitude in the UBV system mag e_Bmag Mean error in Bmag mag apBmag Aperture for Bmag arcsec r_Bmag Reference code for Bmag magnitude number=3 See explanation in file "refs.dat" --- B-V B-V color in the UBV system mag U-B U-B color in the UBV system mag r_B-V Reference to U-B and B-V number=3 See explanation in file "refs.dat" --- RV Radial velocity km/s e_RV Radial velocity mean error km/s r_RV Radial velocity reference number=3 See explanation in file "refs.dat" --- Identifications References ID Identification, see ID in table catalog.dat --- Text Text of bibliographic reference --- Magnitude, Color and Radial Velocity References Code Reference code (columns r_Bmag, r_B-V, r_RV of catalog.dat) --- Data Type of data taken from reference: Z = reference for radial velocity other = magnitude bandpass, e.g. 'UBV' --- Text Text of bibliographic reference --- Notes to catalog RAh Hours RA, equinox 1950 h RAm Minutes RA, equinox 1950 min RAs Seconds RA, equinox 1950 s DE- Sign Dec, equinox 1950 --- DEd Degrees Dec, equinox 1950 deg DEm Minutes Dec, equinox 1950 arcmin ESO ESO/Uppsala identifier --- Text Text of note --- Plate centers Field Field number --- NPC_RAh Hours RA, 1950.0, of nominal plate center h NPC_RAm Minutes RA, 1950.0, of nominal plate center min NPC_DEdeg Degrees Dec, 1950.0, of nominal plate center deg Plate Plate number --- RAh Hours RA, 1950.0, of plate center h RAm Minutes RA, 1950.0, of plate center min RAs Seconds RA, 1950.0, of plate center s DE- Sign Dec, 1950.0, of plate center --- DEd Degrees Dec, 1950.0, of plate center deg DEm Minutes Dec, 1950.0, of plate center arcmin Diff_X Center difference, X mm Diff_Y Center difference, Y mm Exp.Y Exposure start time, year, Universal Time a Exp.M Exposure start time, month, Universal Time --- Exp.d Exposure start time, day, Universal Time d ExpST.h Exposure start time, hour, Sideral Time h ExpST.m Exposure start time, minutes, Sideral Time min Seeing Seeing quality number=1 Seeing judged on a 5-step scale; the corresponding approximate image diameters are as follows: 1 - <25 microns (156 plates) 2 - 20-30 microns (182 plates) 3 - 25-35 microns (141 plates) 4 - 30-40 microns ( 79 plates) 5 - >35 microns ( 48 plates) --- Obs_Code Observer code number=2 the Observer code is: GPA - Guido Pizarro (186 plates) OPA - Oscar Pizarro (180 plates) HES - Hans-Emil Schuster (167 plates) DBA - Dominique Ballereau ( 72 plates) AZU - Alberto Zuniga ( 1 plate ) --- Note Note number=3 the coded notes stand for: 1 - Clouds 2 - Wind 3 - Cirrus 4 - Humidity 5 - Wind and clouds 6 - Image motion 7 - (not used) 8 - No grid on plate (plate number < 400) 9 - Plate not used in ESO/Uppsala Survey. --- Francois Ochsenbein CDS 1998 Jun 30 The authors of the ADC document (Lee E. Brotzman and Robert S. Hill) wish to thank Dr. Lauberts for his assistance in completing the ADC version of the ESO/U catalog. A large fraction of the contents of the "ReadMe" file originates from the "Documentation for the machine-readable version of the ESO/Uppsala Survey of the ESO(B) Atlas", prepared in June 1985 by Lee E. Brotzman and Robert S. Hill at NASA/ADC, document SASC-T-1-5810-5003-85. UNKNOWN UNKNOWN * June 1985, by Lee E. Brotzman and Robert S. Hill: The ESO/U catalog was sent to the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, by the Centre de Donnees Stellaires (CDS), in January 1983. This version was equivalent to the book version of the en- tire catalog (Lauberts 1982), having two records per object and a separate notes file. The following changes were made to the catalog format: o The main catalog file was reformatted to have one record per object. o The object classes were placed into a consistent format. o The flags for additional information were segregated each into its own byte in the record. o The notes file was proofread and notes for individual objects were placed in separate records. Programs were written to compare the main catalog file and the notes file, in order to assure that every note had a corresponding note flag in the main catalog, and vice versa. Discrepancies were checked against the lists published in the A. & A. Suppl., against the errata in the A. & A. Suppl., and against the book version. The results of this comparison and other minor corrections were sent to Dr. Andris Lauberts at Uppsala Observatory for confirmation and approval. With his reply, Dr. Lauberts supplied a tape of the then current version of the ESO/U catalog (dated September 9, 1984). This version had four records per object with a record length of 80 bytes, and had the notes incorporated into the catalog record. The new version allowed changes and updates to be made easily with a standard text editor. The processing of this new version was much the same as the previous one: o The main catalog file was reformatted into one record per object. o The object classes were placed into a consistent format. o The notes were placed into a separate file to keep the record length of the main catalog file to a reasonable size. o The programs to compare the catalog with the notes file were run and no discrepancies between these files remain. o The files containing the references to identifications, the references to magnitudes and radial velocities, and the plate data were made from the documentation file on the tape provided by Dr. Lauberts. * 20-Jul-1993, by F. Ochsenbein, CDS: The following few modifications have been made to the original catalogue from the ADC CD-ROM (NASA, 1991) "Selected Astronomical Catalogs Vol. 1": o File "catalog" was transformed from the ADC CD-ROM file nonstell/galaxies/esoupp/esoupp.dat, and - the field e_Bmag/apBmag (mean error on B or aperture) has been transformed into two columns - the flags in columns 147-148 have been put in the right column - the flags in columns 77 and 81 were corrected to : (colon) for the various characters found (e.g. dots, commas, minus), and also for the 3 galaxies 2-G 4, 423-G 9 and 406-G 5 which had a numeric value in column 81 (6, 3 and 1 respectively) - the Hubble class started in column 86 instead of column 90 for 9 objects at positions 023457-3424.0, 085101-3517.2, 132049-4137.6, 052059-2757.1, 071514-2849.6, 075750-2426.0, 095433-3137.7, 105443-3253.3, 224002-3520.0 - values of 0.00 for e_Bmag were transformed to blanks (unknown) o File "plates": records with a value of "60" in RAs or "60.0" in DEm have been corrected (fields 301, 306, 308, 336, 338, 425, 438, 512) o Other remarks: - Many reference codes are included in "refs" file which never appear in the "catalog" file: AA, 1A, 1D, 3A, 3D, 4A, 5A, 5D, 6A, 7A, 9A, 9D, 9F, 9G, 9H, 9J, 9L, 9M. - r_Bmag for 122732-6557.8 is "FW", which was only in "idrefs" file; it has been added to "refs" file - The statistics of the observer code is not consistent with those in "adc.doc" file. The following modifications have been made: "AZA" changed to "AZU" "BAL" and "BSL" changed to "DBA" "DPA" changed to "GPA" The results obtained from the "plates" file are then, if the 6 additional plates are substrated: AZU(1) DBA(73) GPA(184) HES(167) OPA(181) * Documentation file revisited on 25-Oct-1995 * 08-Jul-1998: it was discovered by Ivan Valtchanov <ivan@astro.bas.bg> that radial velocities larger than 9999 or smaller than -999km/s were truncated to the last four digits. This truncation apparently did not exist in the very original file supplied by A. Lauberts to CDS in 1982, but appears in the 1985 version created at ADC. The 143 velocities concerned where corrected at CDS. Velocities also checked versus Lauberts-Valentijn <VII/115> and PGC <VII/119>, and 122 further corrections on the velocities were performed. VII_34C.xml Detailed bibliography of the surface photometry of galaxies 7039A VII/39A Bibliography of Surface Photometry of galaxies Detailed bibliography of the surface photometry of galaxies E Davoust J D Pence Astron. Astrophys. Suppl. Ser. 49 631 1982 1982A&AS...49..631D Bibliography Galaxies, optical Galaxy catalogs Photometry, surface (adapted from the "Documentation for the Machine-Readable Version of the Detailed bibliography of the surface photometry of galaxies by Lee E. Brotzman and Robert S. Hill (ADC), SASC-T-1-5810-5006-84, July 1984) The bibliography supplies coded information about the methods of observation and reduction, types of photometric data, limiting surface brightness, and the general purpose of each paper for about 650 galaxies and 300 references.
The bibliography of Surface Photometry Name Galaxy name number=1 The name consists of the catalogue designation immediately followed by the catalogue number (except in the case of a commonly used name). The catalogue designations are, in order of appearance: N New General Catalogue (NGC) I Index Catalogue (IC) MK Markarian; galaxies with ultraviolet continuum DDO David Dunlop Observatory dwarf galaxies VV Vorontsov-Vel'yaminov LMC, SMC the Large and Small Magellanic Clouds FORNAXDW, SCULP.DW the Fornax and Sculptor dwarf galaxies A anonymous galaxies not appearing in any of the above catalogues. The number follows the rules given in RC2 U Uppsala General Catalogue of Galaxies (UGC) The last 15 records of the file list the main galaxy clusters which have been studied (excluding Virgo). --- Hubble Revised numerical Hubble type as explained in Section 3.2 of RC2 --- u_Hubble "*"=uncertain, "$"=doubtful, "P"=peculiar, or blank. --- BT The total B magnitude, or the corrected Harvard magnitude as described in Section 3.2 of RC2 mag Ngal Number of galaxies in study. number=2 The Number of galaxies may be larger than the number of galaxies with documented surface photometry in the paper (e.g., Oemler 1976; de Vaucouleurs and Aguero 1973) --- Nplates Total number of plate exposures number=3 Total number of plate exposures available for the galaxy (sometimes several exposures may be made on one plate). This is not always the number of reduced plates, as some may be trailed for orientation (Ables 1971) or used for visual inspection only. --- Scale Plate scale of the observations number=4 Plate scale of the observations: H = high (less than 20 arc seconds per mm); M = medium (between 20 and 50); L = low (over 50). The plate scale is sometimes changed with a focal reducer in works with digital detectors. An asterisk in byte 27 indicates that the plate scale was not given in the paper. --- Source Source of data number=5 Source of data: A = analog two-dimensional measurement of photographic plate (e.g., Joyce-Loebel, Sabatier effect); 1 = one-dimensional digital scans of plate or film; 2 = two-dimensional digital scanning of the plate or counts of silver grains; G = grid of photoelectric photometry measurements; S = photoelectric drift scans; D = digital two-dimensional detector (e.g., CCD, IPCS, Vidicon). An asterisk in byte 31 indicates that the source of the data was not given in the paper. --- Hresol Highest resolution or minimum scanning aperture number=6 Highest and lowest resolution of the photometric maps and profiles, or minimum and maximum scanning apertures in seconds of arc. The aperture size is defined as the length of a side of a square aperture, the geometric mean of the sides of a rectangular aperture, or the diameter of a circular aperture. This resolution has nothing to do with the atmospheric seeing. arcsec Lresol Lowest resolution, or maximum scanning aperture number=6 Highest and lowest resolution of the photometric maps and profiles, or minimum and maximum scanning apertures in seconds of arc. The aperture size is defined as the length of a side of a square aperture, the geometric mean of the sides of a rectangular aperture, or the diameter of a circular aperture. This resolution has nothing to do with the atmospheric seeing. arcsec CalMethod Method of calibrating the magnitude scale zero point. number=7 Method is defined as follows: A = photoelectric aperture photometry; B = brightness of the night sky (measured photoelectrically or on another plate); D = photoelectric drift scans or previously published profiles of the galaxy; E = extrafocal images of standard stars; S = standard stars or other objects; * = unspecified; U = uncalibrated. --- PassBands Photometric passbands number=8 Photometric passbands and corresponding limiting surface brightness (to the nearest magnitude per square arc second). The bands are U, B, V, R, I with an additional column (E) for any narrow emission line band (H ALF, OIII, etc.). Photometric observations in other systems were forced into the closest band (e.g., J plates are listed under the B band). For the few papers which will not fit into this classification scheme we simply list the total number of colours that were observed (e.g. Swaans 1980, Pronik and collaborators). The U, B, V, R, I, and E, bands are given in that order, each one occupying 3 bytes. --- Pub2 Two-dimensional information on galaxy number=9 the two-dimensional information includes: P = photograph; D = isodensity tracing; I = calibrated isodensity tracing or iso-intensity map; N = numerical intensity or colour index map. --- Pub1 One-dimensional intensity profiles number=10 the one-dimensional intensity profiles include: A = major axis; B = minor axis; E = equivalent luminosity profile (i.e. surface brightness versus equivalent radius r* = sqrt(ab); O = other profile: other position angle, azimuthal luminosity profile, colour profiles, profile along spiral arm, colour-colour diagrams of pixels, position angle of isophotes at different intensity levels, etc. --- PhotPurp General purpose of photometric study number=11 This is not intended to be a complete description of the paper, but only an indication of some of the main subjects covered. 1. spatial luminosity distribution; 2. dust lanes, absorption, scattering laws; 3. bulge, disk, arms, etc. decomposition; 4. star formation, stellar populations, metallicity; 5. individual objects: HII regions, globular clusters; 6. nucleus, compact objects; 7. ellipticity of isophotes or isophote twists; 8. outer halos, filaments, intergalactic connections; 9. dynamics, rotation, mass/luminosity, mass models; A. origin, evolution of galaxies; B. tidal interaction; C. spectral energy distribution; D. extragalactic distance scale. --- Ref The reference number=12 The reference is given as the first author, followed by a "+" if there are any coauthors, and the year of publication. If the galaxy name in bytes 1-9 is one which appears in another catalogue, a cross reference to the primary name is listed in this field (e.g. MK190 = N3928) --- Galaxies sorted by Reference Ref Reference, or blank for continuation number= If a galaxy has more than one name, both are included separated by an "=" sign (e.g., I1613=DDO008). Up to three galaxies may be given in a record, each in a 20-byte field starting at byte 21, 41, and 61. --- Names Galaxies from the given reference If a galaxy has more than one name, both are included separated by an "=" sign (e.g., I1613=DDO008). Up to three galaxies may be given in a record, each in a 20-byte field starting at byte 21, 41, and 61. number= If a galaxy has more than one name, both are included separated by an "=" sign (e.g., I1613=DDO008). Up to three galaxies may be given in a record, each in a 20-byte field starting at byte 21, 41, and 61. --- Index by Galaxies Name Galaxy name --- Alias Alias flag, set to "A" if the galaxy has another name --- RecNo1 Corresponding first record number in "main" --- RecNo2 Corresponding last record number in "main" --- Francois Ochsenbein CDS 1995 Jun 13 UNKNOWN UNKNOWN * July 1984 (from ADC) The original tape of the SPG catalogue was supplied to the Astronomical Data Center (ADC), Goddard Space Flight Center, by the Centre Donnees Stellaires (CDS), Strasbourg, France in late 1983. This tape contained the main data file and the reference file, which were modified at the ADC by deleting blank records, deleting heading records that did not conform to the formats detailed above, and stripping off the CDS number placed in the first eight bytes of each record. The two additional index files, galaxies sorted by reference and the index by galaxy, detailed above, were added by the authors of this document at the ADC, and were generated by extracting and sorting certain fields from the original two files. * 13-Jun-1995 (at CDS) The bytes used to express the resolution values Hresol and Lresol have been expanded from F4.0 to F6.1 to accommodate the large numbers. VII_39A.xml The Coma Cluster - I. A catalogue of magnitudes, colours, ellipticities and position angles for 6724 galaxies in the field of the Coma cluster 7042A VII/42A GMP catalogue: galaxies in the Coma cluster The Coma Cluster - I. A catalogue of magnitudes, colours, ellipticities and position angles for 6724 galaxies in the field of the Coma cluster J G Godwin N Metcalfe J V Peach Mon. Not. R. Astron. Soc. 202 113 1983 1983MNRAS.202..113G Clusters, galaxy The catalogue contains isophotal magnitudes, radii, intensity profiles, ellipticities and (b-r) colours for 6724 galaxies with b26.5 < 21.0 mag in a 26.3 degree square area centered on the Coma cluster. The sample is essentially complete to b26.5 = 20.0, with rms deviations in b26.5, r24.75 and (b-r) all about 0.15mag. The plates used in this investigation were all taken with the Palomar 48-inch Schmidt telescope during good conditions in 1976 May.
The catalogue of galaxies, published as Appendix Microfiche MN202/1 and 2 GMP Identification number --- n_GMP "?" indicates a probable galaxy number=1 Metcalfe and Peach subjectively discriminated between galaxies and stars by examination of 14270 images brighter than b26.5 = 21.0. The final list of objects includes 6205 galaxies, 146 double galaxies, and 2 triple galaxies together with 350 probable galaxies and 21 probable double galaxies for a total of 6724 objects. An extensive discussion of the completeness and purity of the search is given in Section 5 of the paper --- Xpos increasing westwards number=2 X and Y positions in arc seconds relative to the approximate center of the cluster, increasing westwards and northwards respectively. The origin of these coordinates is at RA=12h57.3 Dec=+28d14.4'(1950.0). The galaxies are ordered by increasing Xpos. arcsec Ypos increasing northwards number=2 X and Y positions in arc seconds relative to the approximate center of the cluster, increasing westwards and northwards respectively. The origin of these coordinates is at RA=12h57.3 Dec=+28d14.4'(1950.0). The galaxies are ordered by increasing Xpos. arcsec n_b26.5 indicates an overlapped image in b- band --- b26.5 b-band integrated magnitude number=3 The b-band magnitude integrated within the 26.5b mag/arsec2 isophote. This limiting isophote, about 3 percent over the background sky brightness, was chosen for optimum signal-to-noise ratio. The rms deviation in b26.5, based on the repeatability of measurements using different scans of the same plates, is 0.13 mag for images brighter than b26.5 = 20, rising to 0.2 mag in the range 20 <= b26.5 < 21. The external errors are likely to be of order 0.15 mag for images brighter than b26.5 = 20. mag r(b26.5) Isophotal radius in b; rms is 0.5arcsec number=4 The isophotal radius is defined by r = sqrt(A/pi) where A is the area enclosed within the isophote. arcsec n_r24.75 indicates an overlapped image in r- band --- r24.75 r-band integrated magnitude number=5 The r-band magnitude integrated within the 24.75r mag/arcsec2 isophote. This limiting isophote, about 3 percent over the background sky brightness, was chosen for optimum signal-to-noise ratio. The limiting isophotes for the r-band and b-band magnitudes are separated by roughly the mean galaxy color, so that they refer to roughly equal metric areas in a given galaxy. The rms deviation in r24.75 is 0.2 mag for images brighter than r24.75 = 18. The external errors are likely to be of order 0.15 mag for images brighter than b26.5 = 20. A value of 99.99 indicates the r-band magnitude was omitted because of the limited range of surface brightness measurement. mag r(r24.75) Isophotal radius in r; rms is 0.7arcsec. number=4 The isophotal radius is defined by r = sqrt(A/pi) where A is the area enclosed within the isophote. arcsec (b-r) (b-r) color index number=6 The external error in the (b-r) color is likely to be of order 0.15 mag for images brighter than b26.5 = 20. A value of 9.99 indicates that the color was not determined. mag r(b-r) Isophotal radius in (b-r) number=4 The isophotal radius is defined by r = sqrt(A/pi) where A is the area enclosed within the isophote. arcsec eps Ellipticity number=7 The ellipticity is defined by eps = (1-b/a) , where b/a is the axial ratio of the ellipse best approximating the 24r mag/arcsec2 isophote, or, in the event of an overlap, the lowest undisturbed isophote. The typical accuracy is +/-0.1 for images with isophotal diameter r(r24) >= 5 arcsec. A value of 9.9 indicates the ellipticity was not determined. --- PosAngle Position angle of the major axis number=8 The position angle, theta, of the major axis of the ellipse is measured counter-clockwise on the sky from north. This angle is measured to within a few degrees for most images. A value of 999 indicates that the position angle was not determined. deg alpha(b) Slope parameter in b-band number=9 The slope parameter is defined as the slope of the logarithmic brightness residuals of each image against a polynomial representing the standard stellar profile. Its rms dispersion, based on measurements from overlapping scan areas, is about 0.05mag/arcsec. A value of 9.99 indicates the slope parameter was not determined. mag/arcsec gamma(b) Profile indicator number=10 this parameter specifies the amount by which the central surface brightness of the b-band image fell short of that which would have been expected for a stellar image with the same number of points measured. A value of 9.9 indicates that this quantity was not determined. mag N(points) Number of points used to form alpha(b) and gamma(b) --- GP Number in Godwin and Peach (1977) --- [RB67] Number in Rood and Baum (1967,1968) --- Com Comments number=11 in cases where the object is marked as "double" or "triple" the photometric data refer to the combined image of its components. --- Francois Ochsenbein CDS 1995 Aug 18 UNKNOWN UNKNOWN * A tape version of the catalogue was provided by J.G. Godwin to CDS (Centre de Donnees de Strasbourg) in June 1983 * Modifications made by Lee E. Brotzman and Robert S. Hill at the Astronomical Data Center (ADC), Goddard Space Flight Center, in January 1984: to strip off the CDS number in the first eight bytes, strip off the last four bytes (which were always blank), and to insert default values (all nines) into numerical fields without data. A printed document describing the catalogue was generated. * 18-Aug-1995 at CDS: this standardized documentation was done from Lee E. Brotzman and Robert S. Hill's document. VII_42A.xml Wisconsin Soft X-Ray Diffuse Background All-Sky Survey 7043 VII/43 Wisconsin Soft X-Ray Diffuse Backgr All-Sky Surv Wisconsin Soft X-Ray Diffuse Background All-Sky Survey D McCammon D N Burrows W T Sanders W L Kraushaar ApJ 269 107 1983 1983ApJ...269..107M Surveys X-ray sources The catalog contains all-sky survey of the soft X-ray diffuse background and the count-rate data from which the maps were made for the ten flights included in the survey. It contains 40 files in the machine-readable version and includes documentation and utility subroutines. The data files contain different band maps (B, C, M, M1, M2, I, J, 2-6 keV) in a 0 degree-centered Aitoff projection, in a 180-degree-centered Aitoff projection, in a north polar projection, and in a south polar projection. Lookup tables in the form of FITS images are provided for conversion between pixel coordinates and Galactic coordinates for the various projections.
Effective Area Product as a function of energy for the different X-ray bands Energy Photon energy keV Area_B Effective area in the B band cm^2sr Area_C Effective area in the C band cm^2sr Area_M1 Effective area in the M1 band cm^2sr Area_M2 Effective area in the M2 band cm^2sr Area_I Effective area in the I band cm^2sr Area_J Effective area in the J band cm^2sr Area_26 Effective area in the 2-6 keV band cm^2sr Flight 13.049 (PASS3) Flight 13.083 (PASS3) Flight 13.084 (PASS3) Flight 13.102 (PASS3) Flight 13.103 (PASS3) Flight 13.122 (PASS3) Flight 13.137 (PASS3) Flight 25.045 (PASS3) Flight 25.051 (PASS3) Flight 26.061 (PASS3) Flight Flight number --- Minutes Minutes past the hour for the center of the 0.2 s observation min Seconds Seconds past the minute for the center of the 0.2 s observation s Flag Flag word These 6 characters should be interpreted as an 18-bit octal word, with only the least significant (rightmost) 16 bits being used. They contain the following information (bits numbered 1-16 from left to right - most significant to least significant): 1: set to 1 if the observation contains bad telemetry. 2: set to 1 if there are fewer than 50 useful telemetry subframes in the observation (each observation can contain a maximum of 125 subframes for flights 13.083 and 13.102, or 250 for the other flights). 3: set to 1 if the livetime correction is uncertain. 5: set to 1 if the B and/or C band data are definitely contaminated. 6: set to 1 if the B and/or C band data are possibly contaminated. 10: set to 1 if the payload was pointed at the Earth. 11: set to 1 if a B and/or C band source was in the field of view. These are: HZ43, Am Her, the Cygnus Loop, Vela-Puppis SNR's, Sco X-1, and U Gem. 12: set to 1 if the M and/or I band data show evidence for the presence of a source in the field of view. 13: set to 1 if the J and/or 2-6 band data show evidence for the presence of a source in the field of view. 14: set to 1 if the following sources are in the field of view: Sources listed in the 4-th Uhuru catalog with >= 20 4U cps. Vela-Puppis SNR's. Cygnus Loop. Example: The flag word of the first record of file 31 (13.083) is written as: 004000, indicating that bit 5 is set because the B and C band data for that observation are known to be contaminated. Note that records were not cast onto the maps presented in McCammon et al. (1983) if the following flags were set: For the B and C bands: 1, 2, 3, 5, 10, 11 For the M1 through 2-6 bands: 1, 2, 3, 10, 14 --- GLON Galactic longitude deg GLAT Galactic latitude deg RA Right Ascension (B1950) deg Dec Declination (B1950) deg Azimuth Azimuth angle deg Zenith Zenith angle deg Altitude Rocket altitude km N_column Column density of nitrogen atoms along the line of sight in the atmosphere This equals twice the number of nitrogen molecules per cm^2 - calculated from CIRA72 model atmosphere, as described in McCammon et al. cm^-2 O_column Column density of oxygen atoms along the line of sight in the atmosphere This equals twice the number of oxygen molecules plus the number of oxygen atoms per cm^2 - calculated from CIRA72 model atmosphere, as described in McCammon et al. (1983). cm^-2 Ar_column Column density of argon atoms along the line of sight in the atmosphere Calculated from CIRA72 model atmosphere, as described in McCammon et al. (1983). cm^-2 B_azimuth Azimuth angle, relative to the Earth's magnetic field deg B_zenith Zenith angle, relative to the Earth's magnetic field deg Rate_B Count rate in band B for this obs. s^-1 Sigma_B One sigma uncertainty for Rate_B s^-1 Trans_B Atmospheric transmission for band B --- Rate_C Count rate in band C for this obs. s^-1 Sigma_C One sigma uncertainty for Rate_C s^-1 Trans_C Atmospheric transmission for band C --- Rate_M Mount rate in band M for this obs. s^-1 Sigma_M One sigma uncertainty for Rate_M s^-1 Trans_M Atmospheric transmission for band M --- Rate_M1 Count rate in band M1 for this obs. s^-1 Sigma_M1 One sigma uncertainty for Rate_M1 s^-1 Trans_M1 Atmospheric transmission for band M1 --- Rate_M2 Count rate in band M2 for this obs. s^-1 Sigma_M2 One sigma uncertainty for Rate_M2 s^-1 Trans_M2 Atmospheric transmission for band M2 --- Rate_I Count rate in band I for this obs. s^-1 Sigma_I One sigma uncertainty for Rate_I s^-1 Trans_I Atmospheric transmission for band I --- Rate_J Count rate in band J for this obs. s^-1 Sigma_J One sigma uncertainty for Rate_J s^-1 Trans_J Atmospheric transmission for band J --- Rate_26 Count rate in band 2-6 keV for this obs. s^-1 Sigma_26 One sigma uncertainty for Rate_26 s^-1 Trans_26 Atmospheric transmission for band 2-6 keV --- doc_gen.doc General documentation for the survey doc_rate.doc Documentation for the countrate files (p*.dat) programs.doc FORTRAN subroutines for accessing the original data files a0b.fit Aitoff, centered on Galactic center (0 deg), B band a0b_mask.fit Aitoff 0 B band (with contaminated regions defined by the subroutine REMOVE in programs.doc zeroed) a0c.fit Aitoff 0 C band a0c_mask.fit Aitoff 0 C band (with contaminated regions defined by the subroutine REMOVE in programs.doc zeroed) a0m.fit Aitoff, centered on Galactic center, M band a0m1.fit Aitoff 0 M1 band a0m2.fit Aitoff 0 M2 band a0i.fit Aitoff 0 I band a0j.fit Aitoff 0 J band a026.fit Aitoff 0 2-6 keV band a180b.fit Aitoff, centered on anticenter (180 deg), B band a180c.fit Aitoff 180 C band a180m.fit Aitoff 180 deg M band a180m1.fit Aitoff 180 deg M1 band a180m2.fit Aitoff 180 deg M2 band a180i.fit Aitoff 180 deg I band galxy0.fit Aitoff 0 deg mapping of (l,b) to pixels galxy180.fit Aitoff 180 deg mapping of (l,b) to pixels xygal0.fit Aitoff 0 deg mapping of pixels to (l,b) xygal180.fit Aitoff 180 deg mapping of pixels to (l,b) npb.fit North Polar B band npc.fit North Polar C band npm.fit North Polar M band npm1.fit North Polar M1 band npm2.fit North Polar M2 band npi.fit North Polar I band spb.fit South Polar B band spc.fit South Polar C band spm.fit South Polar M band spm1.fit South Polar M1 band spm2.fit South Polar M2 band spi.fit South Polar I band galxy_np.fit Zenithal Equal Area mapping of (l,b) to pixels for North Polar projection galxy_sp.fit Zenithal Equal Area mapping of (l,b) to pixels for South Polar projection xygal_np.fit Zenithal Equal Area mapping of pixels to (l,b) for North Polar projection xygal_np.fit Zenithal Equal Area mapping of pixels to (l,b) for South Polar projection Seth W. Digel and Gail L. Schneider SSDOO/ADC 1997 Oct 09 VII_43.xml Catalogue of Star Clusters and Associations. II. Globular Clusters. 7044B VII/44B Star Clusters & Associations II. Globular Clusters Catalogue of Star Clusters and Associations. II. Globular Clusters. J Ruprecht B Balazs R E White Akademiai Kiado, Publ. House Hungarian Acad. Sciences, Budapest ??? ??? 1981 1981 Catalogue of Star Clusters and Associations. II. Globular Clusters. J Ruprecht B Balazs R E White Soviet Astronomy 27 358 1983 1983SvA....27..358R VII/5 : Excerpt from the Catalogue of Star Clusters and Associations VII/31 : Part I: Associations VII/101 : Part III: Open Clusters VII/103 : Catalogue of galactic globular clusters by R. Monella, 1985, VII/151 : Structure parameters of galactic globular clusters by R.F. Webbink, 1985, in IAU Symp. 113 "Dynamics of star clusters", Ed. J. Goodman & P. Hut, 541 Alter G., Ruprecht J., and Vanysek V., 1970, "Catalog of Star Clusters and Associations", 2nd edition, Akad. Kiado, Budapest. Clusters, globular The catalog is the complete bibliographical listing for globular clusters from the second edition of the "Catalogue of Star Clusters and Associations (CSCA)" edited by Alter et al. (1970), and the "Supplement to the CSCA" by Ruprecht et al. (1981). Thus, it covers the literature through 1973. The file "main.dat" contains the original data: for each cluster, the first line contains the running number (GCL) followed by designations used by various authors; the second line contains the 1950 coordinates, the 50-yr precession, the galactic coordinates, the galactic direction cosines and the position on the POSS charts; the lines following provide the following parameters: YEAR: Year of the literature reference NAME: Author PUBLICATION: Reference AD: Apparent diameter of the cluster (arcmin) DIST: Distance of the cluster (pc) LD: Linear diameter of the cluster (pc) N: Number of stars studied CE: Color excess SP: Integrated spectrum RV: Radial velocity (km/s) MT: Total (integrated) magnitude NOTE: Notes The file "clusters.dat" has been created from second lines; missing positions were filled with the help of the SIMBAD data-base <http://cdsweb.u-strasbg.fr/Simbad/html>.
List of globular clusters GCl Cluster name (starting with GCL) --- Page Card (or page) number of the second edition --- Name Other name of the cluster --- RAh Right Ascension 1950 (hours) number=1 the position was added at CDS for additional clusters, i.e. GCL names with decimal figures. h RAm Right Ascension 1950 (minutes) number=1 the position was added at CDS for additional clusters, i.e. GCL names with decimal figures. min DE- Declination 1950 (sign) number=1 the position was added at CDS for additional clusters, i.e. GCL names with decimal figures. --- DEd Declination 1950 (degrees) number=1 the position was added at CDS for additional clusters, i.e. GCL names with decimal figures. deg DEm Declination 1950 (minutes) number=1 the position was added at CDS for additional clusters, i.e. GCL names with decimal figures. arcmin GLON Galactic longitude number=1 the position was added at CDS for additional clusters, i.e. GCL names with decimal figures. deg GLAT Galactic latitude number=1 the position was added at CDS for additional clusters, i.e. GCL names with decimal figures. deg POSS Palomar Sky Survey chart with its RA and Dec --- Xpos Position on the Palomar chart from lower left corner mm Ypos Position on the Palomar chart from lower left corner mm main.txt Bibliography of globular clusters Francois Ochsenbein CDS 1995 Nov 02 UNKNOWN UNKNOWN * November 1983: Tape provided to CDS by Moscow Data Centre * in 1985: description of the machine-readable version provided by Dr Ch. Peterson, Univ. California, Berkeley. * October 1991: CD-ROM edition "Selected Astronomical Catalogs" Vol. 1 by ADC/GSFC, directory /nonstell/clusters/globular * 06-Jul-1994: Addition of "clusters" file at CDS * 02-Nov-1995: "ReadMe" file revisited at CDS * 11-Nov-1996: Ypos data for GCL-100 2929 Pal 8 were "73 " changed to " 73" without checking. VII_44B.xml Seyfert Galaxies 7047 VII/47 Seyfert Galaxies Seyfert Galaxies D W Weedman Ann. Rev. Astron. Astrophys. 15 69 1977 1977ARA&A..15...69W Galaxies, Seyfert Galaxy catalogs This catalog is a combination of two Seyfert galaxy lists published by Weedman in 1977 and 1978. This version includes 121 objects, 88 from the first published list and 33 from the second. The lists are merged and sorted by right ascension. The criteria for objects to be included are the same for both lists and are as follows: broad emission lines, non-stellar (nebulous) appearance on Palomar Sky Survey prints ("This means in practice that it must have a diameter greater than about 7" for the nebulosity around the nucleus to be visible."), and Seyfert designation in a published reference (no unpublished Seyferts included). Also, the lists omit "galaxies referred to by spectroscopists as probably or possibly being Seyferts unless UBV photometry also showed the characteristic Seyfert colors." (Weedman's italics.) Also, quasars are excluded. In the introduction to the second list, Weedman remarks that four galaxies from the first list were not confirmed spectroscopically as Seyfert (Phillips M.M., and Osterbrock D.E., 1977. Publ. Astron. Soc. Pacific, 89, 251) and "should be deleted..." However, these have been retained in the machine-readable version in order to conform to the lists as published. These galaxies are as follows: AKN 42, AKN 81, AKN 223, and AKN 253. The catalog lists for each Seyfert designation of object, list reference number, equatorial position and positional accuracy, redshift, angular major axis, B-V and U-B color indices, references to UBV photometry, spectra, and radio data. The second list did not include angular major axis and color indices.
Catalog Data Name Designation of object --- list 1 = from 1977 list; 2 = from 1978 list --- RAh Right Ascension (epoch 1950.0) hours h RAm Right Ascension (epoch 1950.0) minutes min RAs Right Ascension (epoch 1950.0) seconds s u_RAs Code for accuracy of Right Ascension 1 = originally to 0.1 minute 2 = originally to 1 second 3 = originally to 0.1 second --- DE- Declination (epoch 1950.0) sign --- DEd Declination (epoch 1950.0) degrees deg DEm Declination (epoch 1950.0) arcminutes arcmin DEs Declination (epoch 1950.0) arcseconds arcsec u_DEs Code for accuracy of Declination 1 = originally to 0.1 hour 2 = originally to 1 minute 3 = originally to 0.1 minute 4 = originally to 1 second --- class Class of galaxy (1, 1A, 2, 2A) --- cz Redshift km/s ama Angular major axis Angular Major Axis, Measured on Palomar Sky Survey prints by Weedman. (Other photographs used for a few southern objects.) Not given for objects published in the second (1978) list arcsec ref1 References for chart --- B-V B-V color index mag U-B U-B color index mag ref2 References for UBV photometry --- ref3 References for spectra --- ref4 References for Infrared, Radio data --- References ref Reference number as in seyfert.dat --- text Text of reference If ref is blank, then text is continued from the previous record. --- seyfert.doc Documentation Julie Anne Watko SSDOO/ADC 1997 Jan 10 UNKNOWN UNKNOWN The two Seyfert galaxy lists of Weedman (see references below) were keypunched at NASA/Goddard Space Flight Center. The data tables were combined in a uniform format. The bibliographies were also combined, and the reference numbers in the data tables edited accordingly. In the machine- readable version, the precision of the equatorial coordinates is indicated by numerical codes rather than by the usual typographical conventions (which are used in the original tables). Acknowledgement is made to Priscilla Struthers for the initial formatting and keypunching of machine-readable version. The original documentation for this catalog was prepared by Robert S. Hill and Theresa A. Nagy (January 1981). VII_47.xml Catalogue of Galaxies and Clusters of Galaxies, I 7049 VII/49 Galaxies and Clusters of Galaxies Catalogue of Galaxies and Clusters of Galaxies, I F Zwicky E Herzog P Wild Vol. I Pasadena California Institute of Technology ??? ??? 1960 1960 Catalogue of Galaxies and Clusters of Galaxies, I F Zwicky E Herzog Vol. II Pasadena: California Institute of Technology ??? ??? 1963 1963 Catalogue of Galaxies and Clusters of Galaxies, I F Zwicky E Herzog Vol. III Pasadena: California Institute of Technology ??? ??? 1966 1966 Catalogue of Galaxies and Clusters of Galaxies, I F Zwicky E Herzog Vol. IV Pasadena: California Institute of Technology ??? ??? 1968 1968 Catalogue of Galaxies and Clusters of Galaxies, I F Zwicky M Karpowicz C T Kowal Vol. V Pasadena: California Institute of Technology ??? ??? 1965 1965 Catalogue of Galaxies and Clusters of Galaxies, I F Zwicky C T Kowal Vol. VI Pasadena: California Institute of Technology ??? ??? 1968 1968 Galaxy catalogs This document describes a machine-readable version of a portion of the "Catalogue of Galaxies and Clusters of Galaxies" (Zwicky, et al.). The published catalogue covers 560 Palomar Sky Survey fields, and for each field it lists both individual galaxies and clusters of galaxies. Its limiting magnitude for galaxies is approximately +15.5 apparent photographic magnitude. The present machine-readable version includes only the individual galaxies. It consists of two files, the first of which lists the galaxies (data file) and the second of which enumerates the fields covered (headers file). Note: the abbreviation ADC used in this document refers to the Astronomical Data Center, NASA/Goddard Space Flight Center. Foreword: All this documentation file is derived from the "Documentation for the Machine-Readable Version of the Catalogue of Galaxies and Clusters of Galaxies: Data on Individual Galaxies" prepared by Robert S. Hill, NASA Doc. SSD-T-1-5069-0022-82 (November 1982)
Data on individual galaxies Field Field number number=1 not all the fields surveyed are represented in this file, as some contain clusters only. The fields coincide with a subset of Palomar Sky Survey fields but are numbered differently. The records in this file are sorted in the same order as the corresponding data in the published catalogue: by field number (ascending), and within each field by right ascension (ascending). --- RAh Hours RA, 1950.0 of the field center h RAm Minutes RA, 1950.0 of the field center min DE- Sign Dec, 1950.0 --- DEd Degrees Dec, 1950.0 of the field center deg DEm Minutes Dec, 1950.0 of the field center arcmin Pmag Apparent photographic magnitude number=2 The introduction to vol. 1 of the published catalogue contains detailed descriptions of the methods of estimation, which can be summarized as follows: magnitudes down to about 15.2 or 15.5 were estimated using the Schraffier method on films taken with an 18-inch Schmidt camera; below this magnitude range, estimates were made directly from the 48-inch Schmidt plates. The nominal limiting magnitude of the catalogue is +15.7, but fainter objects may be present. mag Rem_Code '1' if remark in published version number=3 Remarks include notations such as "diffuse" or "compact." Numerical data, such as velocities or Harvard magnitudes, are not taken to be remarks. --- Headers (fields) Field Field number number=1 All the published fields are represented in this file, with one record per field, even if the field contains no individual galaxies. The field center may be displaced from the corresponding Palomar Sky Survey plate center by as much as half a degree, but the entire field is always contained within the corresponding Palomar Sky Survey plate area. The fields are six by six degrees. --- RAh Hours RA, 1950.0 of the field center h RAm Minutes RA, 1950.0 of the field center min DE- Sign Dec, 1950.0 --- DEd Degrees Dec, 1950.0 of the field center deg DEm Minutes Dec, 1950.0 of the field center arcmin GalCnt Galaxy count for field number=2 This information was generated by computer and is not in the published catalogue. The following fields contain no individual galaxies (headers are, however, present in this file): 443 444 489 490 509 510 511 527 528 543 --- POSS Palomar Obs. Sky Survey plate number number=3 This information was derived independently of the published catalogue by comparison with a Fortran program of center coordinates to a PSS headers file (see Catalogue: VI/25) --- MLP Mead-Luyten-Palomar number number=4 This system numbers the PSS fields (including Whiteoak extension) from 1 ... 1037. The numbers equal the corresponding Luyten- Palomar (LP) numbers plus 1, except for the north polar fields, which in the LP system are numbered 1A and 1B; and in the MLP system, 1 and 2. The LP system comes from the Luyten- Palomar automated proper motion survey. The MLP numbers are used in PSS-oriented catalogues developed by the ADC. --- Francois Ochsenbein CDS 1995 Oct 02 UNKNOWN UNKNOWN * November 1982, by Robert S. Hill (Doc. SSD-T-1-5069-0022-82) This version is based on one supplied to the ADC by M. Hauser (NASA/GSFC), which consists of six files of card images corresponding to the six volumes of the published catalogue. For each survey field, there is a header record and a trailer record, and the data for the galaxies are in the intervening records, with four galaxies per record. According to Hauser (private communication), this version may have been keypunched at the California Institute of Technology in the early 1970's. The present version was generated by the following steps: (1) the information for each galaxy was written to a separate record, to which the field number was added; (2) the header and trailer records were deleted, and the headers were written to a separate file; (3) using a Fortran program, the headers were compared to data on the Palomar Sky Survey fields, and the PSS and MLP numbers were added as appropriate; (4) the galaxy counts for each field were generated and added to the headers. In addition, the following errors were corrected: (1) thirteen galaxies dropped from field 30 were restored; (2) the errata published in vols. 2-6 were incorporated as far as they were relevant, as follows: Field No. Correction 13 Galaxy 1156.7-0323 became 1158.7-0323. 39 Galaxy 1118.6+0328 added. 41 Galaxy 1212.7+0602 added. 42 Galaxy 1221.1+0720 got remarks flag. 42 Galaxy 1221.2+0728 became 1221.3+0728. 42 Galaxy 1221.5+0719 became 1221.6+0719. 70 Galaxy 1223.7+1314 Lost remarks flag. 70 Galaxy 1223.9+0917 got remarks flag. 70 Galaxy 1228.0+1246 added. 126 Galaxy 1110.8+2226 added. 153 Pmag of galaxy 956.4+3059 became 13.6. 267 Galaxy 1100.0+5629 became 1100.2+5629. 431 Pmag of galaxy 2326.0+1427 became 13.2. Not all the data on individual galaxies in the original published catalogue are in this version. In particular, there are no IC or NGC numbers, velocities, or data from other catalogues. Also, supplementary data on particular galaxies within the clusters are not included. * November 1991: on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM, directory /nonstell/galaxies/cgcg * October 1995: documentation standardized at CDS VII_49.xml Catalog of CO Radial Velocities toward Galactic H II Regions 7050 VII/50 CO Radial Velocities Toward Galactic H II Regions Catalog of CO Radial Velocities toward Galactic H II Regions L Blitz M Fich A A Stark Astrophys. Journ. Suppl. 49 183 1982 1982ApJS...49..183B Catalog of CO Radial Velocities toward Galactic H II Regions A R Gillespie P J Huggins T C L G Sollner T G Phillips F F Gardner S H Knowles Astron. and Astrophys. 60 221 1977 1977A&A....60..221G Radial velocities H II regions Carbon monoxide Galaxy catalogs The catalog contains machine-readable versions of the "Catalog of CO Radial Velocities Toward Galactic HII Regions" (Blitz et al. 1982) and the "Catalog of Carbon Monoxide Observations of Southern Hemisphere HII Regions" (Gillespie et al. 1977) in two separate files. The former is a catalog of 242 molecular cloud complexes that are associated with optical HII regions and includes source names, coordinates, CO radial velocities, antenna temperatures and full width at half-maximum at the position of the strongest CO emission, references for the observations, distances to the stars exciting the HII regions, and optical diameters of the HII regions. The latter is the first CO survey of the southern sky; it was made using the Anglo-Australian 3.9-m optical telescope at 115 GHz (2.6-mm wavelength) with a hot-electron bolometer receiver located at the Coude focus. The data were collected during two observing periods (September 1975, April 1976) and include designations, coordinates, median values for the velocities, and distances to the stars exciting the HII regions.
CO Radial Vel. toward Galactic H II regions ID Source name Source name. This file contains data for 294 sources from the Sharpless catalogue and 67 additional sources (33 of which had not been previously catalogued) that were found by the authors on Palomar Sky Survey (PSS) prints. Sharpless objects are indicated by an 'S' in byte 1, followed immediately by the catalogue number. The additional HII regions are denoted by 'BFS' in bytes 1-3, followed immediately by a sequence number. The initial magnetic tape contained data for two other sources not presented in the published catalogue. The sources are included in this version and have 'BFS' in bytes 1-3 without a sequence number. The records in this file have been sorted by galactic longitude, l(II) (bytes 28-33). --- RAh Right ascension (equinox B1950) Hours Equatorial coordinates (1950) of the approximate center of light of the HII region. h RAm RA Minutes min RAs RA Seconds s DE- Sign of Declination (equinox B1950) --- DEd DEC Degrees of arc deg DEm DEC Minutes of arc arcmin GLON1 Galactic longitude, l(II) center region Galactic coordinates (system II, 1950) of the approximate center of light of the HII region. The file is sorted on GLON1 field. deg GLAT1 Galactic latitude, b(II) deg Lflag1 uncertainty flag '(' or ')' if the association of the CO emission with the HII region is uncertain. --- RV Observed value of radial velocity CO radial velocity. This gives the velocity centroid of the CO emission weighted by the intensity at each location at which the detection was made. The uncertainty given is a 1 sigma formal error of the intensity-weighted velocity centroid for all of the detected lines. Several different no-data flags are provided with the following explanations: 999.9 - "No detection". No CO was detected at any of the positions observed to the limit of sensitivity (typically 0.5K). 888.8 - "No definite detection". Weak emission was observed which is probably unrelated to the HII region. 777.7 - "Cannot associate". Relatively strong emission was detected which could not definitely be associated with the HII region. 666.6 - "No observation". 555.5 - "Needs extensive mapping". If one of the above flags appears in bytes 43-47, the data in bytes 48-80 should be ignored. km/s u_RV Uncertainty of radial velocity measurement --- Rflag1 uncertainty flag --- Lflag2 uncertainty flag --- AntTemp Antenna temperature Antenna temperature at the position of the strongest CO emission. Because, in general, the CO emission was not mapped, this may not be the peak CO temperature in the cloud complex. The peak antenna temperatures should generally be accurate to at least 25 percent and in most cases to 10 percent. K Rflag2 uncertainty flag --- Lflag3 uncertainty flag only for BFS42 '(' if there is uncertain association (see bytes 42 and 53), or '<' indicating the value in byte 62-65 is an upper bound. For one source, BFS42, both of the above conditions exist and bytes 60-61 are '(' and '<', respectively. --- Lflag32 uncertainty flag with one exception --- FWHM Full width at half-maximum Full width at half-maximum, in km/s, of the strongest CO line. This quantity was measured directly from the profiles and is not based on Gaussian fitting because of the complex nature of many of the profiles. km/s Rflag3 uncertainty flag --- GLON2 Galactic longitude, l(II) of center strongest CO line Galactic coordinates (system II, 1950) of the position of the strongest CO line. This position rarely differs from the position in bytes 28-40 by more than the radius of the HII region. deg GLAT2 Galactic latitude, b(II) deg ref CO references CO references for the observation presented in the catalogue. If more than one reference is given, the parameters of the CO line at the peak position are generally taken from the most extensive or well-sampled observations. The list of numbers in this field refer to those records of file 3, ntesrefs.dat, Notes and References, with an 'R' in byte 1. --- Lflag4 '(' uncertainty flag concerning distance --- Distan Distance Distance, in kpc, to the star exciting the HII region. This was determined by spectrophotometry of the stars and all cases are taken from the published literature. kpc e_Distan Error of distance in kpc kpc Rflag4 uncertainty flag concerning distance --- RefNum Reference numbers contained in parentheses The list of numbers in this field refer to those records of file 3, Notes and References, with an 'R' in byte 1. --- OptDiam Optical diameter of the HII region Taken from the Sharpless catalogue and from measurements of the red PSS prints for the newly catalogued sources. arcmin DegMap Degree of mapping toward the HII region Degree of mapping toward the HII region as follows: P = partial, E = extensive, C = complete. A blank in this column means only a few points have been observed. --- RefMap Reference numbers for the mapping contained in parentheses. --- note Comments. Comments. This area gives other identifications for the HII region and associated objects and an indication if there is additional material in file 3 (ntesrefs.dat), Notes and References (the string '(NOTES)' will appear if this is the case). For the additional sources found by the authors and denoted by 'BFS' in bytes 1-4, references to other catalogues are as follows: BER = Bernes 1977, DG = Dorschner and Guertler 1963, LBN = Lynds 1965, M = Marsalkova 1974, PK = Perek and Kohoutek 1967, PP = Parsamian and Petrossian 1979, RCW = Rogers, Campbell, and Whiteoak 1960. VDB = van den Bergh 1966, --- CO at Southern Hemisphere H II Regions Sname Source designation. Source designation. Names have been given for 24 of the 37 sources appearing in this file. NGC = Sulentic and Tifft 1973, RCW = Rogers, Campbell, and Whiteoak 1960, W = Westerhout 1958. --- RAh Right Ascension (Equatorial coord. 1950) h RAm RA Minutes min RAs RA Seconds s DE- Sign, always '-', of Declination --- DEd DEC Degrees of arc (equinox 1950) deg DEm DEC Minutes of arc arcmin GLON Galactic longitude, l(II), in degrees Galactic coordinates (System II, 1950) of the observation. deg GLAT Galactic latitude, b(II), in degrees deg VLSR Median CO velocity (Local Standard of Rest) km/s EW Equivalent line width, in km/s. Defined as (Integration of TA* over dv)/TA* (max) where TA* is the corrected antenna temperature, bytes 63-66. km/s PAtt-tem Peak antenna temperature Peak antenna temperature, TA*, corrected for atmospheric extinction and telescope efficiency. K CAtt-tem Continuum antenna temperature at 5 GHz, Tc Continuum antenna temperature at 5 GHz, Tc. This value was taken from Whiteoak and Gardner 1974. K V-H109 Velocity of the H 109 alpha line Comparison values for the velocities of the H 109 alpha line and the strongest OH and H2CO lines (Wilson, et al. 1970, Whiteoak and Gardner 1974, Caswell and Robinson 1974). These values will be 0.0 if no data are available. For V-OH3, a value is available only for the source listed in record 27, all other records have 0.0 in this field. km/s V-OH1 Velocity of the OH line km/s V-OH2 Velocity of another strong OH line km/s V-OH3 Velocity of another strong OH line km/s V-H2CO1 Velocity of the H2CO line km/s flag1 '(' - uncertainty about the V-H2CO2 data --- V-H2CO2 Velocity of another strong H2CO line km/s flag2 ')' - uncertainty about the V-H2CO2 data --- Distan Distance Distance to the star exciting the HII region, in kpc. This value is 0.0 if no distance is available. kpc e_Distan Error of distance measurement kpc Com Notes This field contains a list of letters A through E separated by commas. The note inferred by each letter may be found in File 3 - Notes and References by finding that letter in byte 1. --- Notes & References DataInd Data type indicator Data type indicator. The character found in this byte determines how the data in the rest of the record should be viewed. The characters used as indicators are listed below in order of appearance in the file (the term 'data field' in the definitions refers to bytes 6-72 of the record): S - The data field is a note for an object from the Sharpless catalogue which was observed by Blitz, Fich, and Stark. These objects are indicated in file 1 by 'S' in byte 1. See cdradvel.dat, bytes 1-6. Blank - The data field is a note for an object found by Blitz, Fich, and Stark. These objects are indicated in file 1 by 'BFS' in bytes 1-3. See cdradvel.dat, bytes 1-6. A,B,C,D,E - The data field is a note for an object observed by Gillespie, et al. and listed in file 2. See cosoreg.dat, bytes 134-138. R - The data field is a reference mentioned in the catalogue of Blitz, Fich, and Stark. See cdradvel.dat, bytes bytes 82-88, 102-108, and 120-126. The character '+' is used to indicate that the data field is a continuation of the previous record. --- RefNum Object or reference number Object or reference number. If byte 1 contains 'S' or is blank, this number is the catalogue number of the object as described in cdradvel.dat, bytes 1-6. If byte 1 contains 'R', this number is the reference number as described in cdradvel.dat, byte 82-88, 102-108, 120-126. --- Dfield Data field Data field. This field contains the notes and references to the catalogues in files cdradvel.dat and cosoreg.dat. --- C.-H. Joseph Lyu Hughes STX/NASA 1996 Jul 17 The original ADC documentation by Lee E. Brotzman and Robert S. Hill (1983) was used to create this ReadMe file. UNKNOWN UNKNOWN The initial magnetic tape version of the catalogues described in this document was supplied by Dr. M. Hauser, Code 693, Goddard Space Flight Center, who obtained the tape from Dr. M. Fich. This tape contained the major parts of the catalogue of Blitz, Fich, and Stark (1982) (BFS), and the catalogue of Gillespie, et al. (1977) combined into one file. The file included the source name, equatorial and galactic coordinates of the HII region, distance of the HII region and the uncertainty in distance, CO radial velocity and the uncertainty in velocity, and the angular diameter of the HII region. The observational results of the two sets of authors were separated into the two files described above in cdradvel.dat and cosoreg.dat. The additional material that was in the published catalogues but not on the initial tape was keypunched at GSFC and merged into their respective files. Finally the third file, Notes and References, was keyed in by Brotzman and Hill. The equatorial and galactic coordinates of the center of light in the BFS file (bytes 7-40) were checked against each other with a Fortran program. Some discrepancies were found. Corrections were supplied by Blitz (1983) and were incorporated into the machine-readable version. These corrections are listed in Table 1. The coordinates of the peak CO position (bytes 68-80) reflect corrections for two objects, which are also given. The round-off errors had been introduced into several of the published galactic coordinates. Although these errors were of no practical importance, recalculated values were substituted for the sake of consistency. Table 1. Errata in Blitz, Fich and Stark (1982) file PUBLISHED MACHINE-READABLE VALUE VALUE OBJECT DATUM (ERRATUM) (CORRECTION) S18 RA 17 44 36 17 44 18 S26 RA 17 54 30 17 55 18 DEC -23 20 -23 26 l 6.10 6.19 b 0.56 0.35 S30 RA 17 59 36 17 59 30 l 7.04 7.03 b -0.26 -0.28 S61 RA 18 30 18 18 30 42 DEC -5 2 -5 1 l 26.36 26.44 b 1.82 1.74 S143 DEC 58 0 57 30 l 107.29 107.23 b -1.43 -1.34 S195 RA 2 36 6 2 36 18 l 136.36 136.28 b -0.38 -0.41 S200 RA 3 2 30 3 6 30 b 4.12 4.11 S220 RA 4 58 0 3 58 0 DEC 46 16 36 16 l 160.76 160.31 b -12.27 -12.34 S238 RA 4 19 42 4 19 6 S265 RA 5 15 54 6 7 24 DEC 7 23 13 20 l 195.08 196.39 b -16.78 -2.86 BFS17 b(CO) 0.21 0.02 BFS18 b(CO) 0.16 0.02 BFS20 RA 0 31 2 0 31 39 l 121.48 121.45 VII_50.xml Revised Shapley-Ames Catalog of Bright Galaxies 7051 VII/51 Revised Shapley-Ames Catalog of Bright Galaxies Revised Shapley-Ames Catalog of Bright Galaxies A Sandage G A Tammann Carnegie Institution of Washington Publication 635 ??? ??? 1981 1981QB857.S26...... Galaxy catalog *** No Description Available ***
The Catalogue Name Galaxy identification --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Type1 Codes for galaxy types number=1 The codes for galaxy types are made of the following bytes: +0 (22) 'C' cD galaxy 'D' dwarf for E, S0, S and I 'M' merged 'P' pseudo outer ring 'R' outer ring '?' ? +1 (23) 'U' the preceding description is in parentheses (uncertain) '?' ? +2 (24) Code for main galaxy type: 'D' cD galaxy 'P' peculiar 'E' E 'F' E/S0 'K' S0/E 'L' S0 'S' S (S0/a-Sm) 'I' I (for Im or amorphous = I0) '-' E-S0, amorphous '+' S0/a-Im +3 (25) Code for description of bar: 'A' no bar 'B' bar 'X' either S/SB or SAB 'Y' S(B) +4 (26) Code for index that follows S0: '1' 1 '2' 1-2 '3' 2 '4' 2-3 '5' 3 '6' 1-3 +5 (27) Ellipticity of S0 [in () following S0 and index, e.g. E/S0(2/3)(4)] (for E/S0, S0/E, S0, S0/a) '1' ( 1) '2' ( 2) '.' . '9' ( 9) 'Z' (10) +6 (28) Inner ring structure: 'S' (s) 'R' (r) 'T' (rs) 'Q' (sr) +7 (29) Further description of main galaxy type, cases (a) = ellipticity for E (e.g. E4, E5/S0, ...) (b) = spirality for S (same as RC2) : (a) (b) '0' E0 S0/a '1' E1 Sa '2' E2 Sab '3' E3 Sb '4' E4 Sbc '5' E5 Sc '6' E6 Scd '7' E7 Sd '8' Sdm '9' Sm (Im) +8 (30) Code for further description (byte +7) ':' followed by : '?' followed by ? 'U' in () +9 (31) ':' whole type is uncertain '?' ? following whole type 'U' whole type in parentheses () 'V' whole type in brackets [] +10 (32) 'P' pec 'B' (pec) 'F' pec: 'G' pec? --- op For double descriptions (if second type mentioned) 'R' (or) '+' (and) --- Type2 Description of second type number=1 The codes for galaxy types are made of the following bytes: +0 (22) 'C' cD galaxy 'D' dwarf for E, S0, S and I 'M' merged 'P' pseudo outer ring 'R' outer ring '?' ? +1 (23) 'U' the preceding description is in parentheses (uncertain) '?' ? +2 (24) Code for main galaxy type: 'D' cD galaxy 'P' peculiar 'E' E 'F' E/S0 'K' S0/E 'L' S0 'S' S (S0/a-Sm) 'I' I (for Im or amorphous = I0) '-' E-S0, amorphous '+' S0/a-Im +3 (25) Code for description of bar: 'A' no bar 'B' bar 'X' either S/SB or SAB 'Y' S(B) +4 (26) Code for index that follows S0: '1' 1 '2' 1-2 '3' 2 '4' 2-3 '5' 3 '6' 1-3 +5 (27) Ellipticity of S0 [in () following S0 and index, e.g. E/S0(2/3)(4)] (for E/S0, S0/E, S0, S0/a) '1' ( 1) '2' ( 2) '.' . '9' ( 9) 'Z' (10) +6 (28) Inner ring structure: 'S' (s) 'R' (r) 'T' (rs) 'Q' (sr) +7 (29) Further description of main galaxy type, cases (a) = ellipticity for E (e.g. E4, E5/S0, ...) (b) = spirality for S (same as RC2) : (a) (b) '0' E0 S0/a '1' E1 Sa '2' E2 Sab '3' E3 Sb '4' E4 Sbc '5' E5 Sc '6' E6 Scd '7' E7 Sd '8' Sdm '9' Sm (Im) +8 (30) Code for further description (byte +7) ':' followed by : '?' followed by ? 'U' in () +9 (31) ':' whole type is uncertain '?' ? following whole type 'U' whole type in parentheses () 'V' whole type in brackets [] +10 (32) 'P' pec 'B' (pec) 'F' pec: 'G' pec? --- Rem Remarks number=2 the remarks are 'D' (dust) 'J' (jet) 'L' (late) 'M' (merged) 'N' (nearly on edge) 'O' (on edge) 'P' (prolate) 'R' (ring) 'T' (tides) 'V' (very early) --- u_Rem '?' for ? --- Lum Luminosity class number=3 the Luminosity class is coded as follows: '1.0' I '1.5' I-II '2.0' II '2.5' II-III '3.0' III '3.5' III-IV '4.0' IV '4.5' IV-V '5.0' V '2.2' II.2 (intermediate classes) '3.2' III.2 etc. --- LumC Luminosity class code number=4 the Luminosity class code is defined as follows: ':' luminosity class followed by : 'U' luminosity class enclosed in () 'V' luminosity class in form (LC): 'W' luminosity class in form (LC:) --- left Left bracket --- B(T) Apparent magnitude B(T) mag u_B(T) Right bracket --- A(i) Internal absorption A(i) mag n_A(i) '*' for special values of A(i) --- Member Group or cluster membership (see Table 2, p. 10 of published catalog) Codes L, S, N, C, M, V, VR, F --- Vel Mean weighted velocity from all available determinations (km/s) km/s e_Vel error in velocity km/s CDS 1995 Feb 08 Original description prepared by: Wayne H. Warren Jr. Astronomical Data Center National Space Science Data Center Greenbelt, Maryland 20771 USA 1987 April This "ReadMe" file was later standardized at CDS. UNKNOWN UNKNOWN The machine-readable catalog was prepared by Dr. R. Kraan-Korteweg of the Astronomisches Institut der Univ. Basel, who graciously supplied it on magnetic tape to Ms. Lynn S. Fischer of the Jet Propulsion Laboratory to be used for the IRAS project. Ms. Fischer kindly supplied it to the Astronomical Data Center (ADC). The machine version was supplied "as is" to Dr. Herbert J. Rood of the Institute for Advanced Study, who checked certain data fields against the published catalog and made suggestions for improvement of the computer version. Modifications made at the ADC include the correction of several errors noted by Dr. Rood, the right justification and alignment of all galaxy designations, the removal of decimal points from some RA values to allow uniform computer processing, and the expansion of the field containing the mean error of the observed velocities to allow for fractional values (these had been rounded) plus the insertion of the correct values. Zero values in the A(i) field were changed to 0.00 so that the field can be read with an F format (there are blank fields also) and the velocity field was expanded so that signs could be moved to occur uniformly in byte 66; "+" signs were added to positive values. A brief description of the data fields in the machine version of the catalog follows. The description has been prepared at the ADC using a handwritten description from Dr. Krann-Korteweg and the data description given in the published catalog (see the latter for more detailed descriptions and comments). This description is brief and almost certainly not complete, since it was assembled from available information without a thorough comparison of the machine version with the published catalog. Any codes not described in the table should be interpreted by comparison with the published catalog. A few coding errors were found and corrected at the ADC during the course of this work, but a complete check has not been made; thus, the ADC takes no responsibility for any errors found. VII_51.xml List of Positions of All X-Ray Sources with Positions Known More Accurately than those Given in the 4U or 2A Catalogues, 2nd Edition 7055 VII/55 X-Ray Source Pos More Accurate than 4U or 2A, 2nd ed. List of Positions of All X-Ray Sources with Positions Known More Accurately than those Given in the 4U or 2A Catalogues, 2nd Edition J F Dolan NASA/GSFC, private communication ??? ??? 1983 1983 VII/12 : This catalog supersedes cat# 7012. Dolan, J. F., 1983, private communication. Nautical Almanac Office, United States Naval Observatory, 1983, The Astronomical almanac (United States Government Printing Office). Astrometric data X-ray sources This catalog is a superset of the X-ray position list in the Astronomical Almanac (1983). It is designed as an aid to observers. Either one or two positions are given for each x-ray source. Identified counterparts are included for many sources.
Uhuru, Ariel
X-ray position list ID Number of the source in the Uhuru 4U Catalog --- Alt Other names of the source Other names of the source, separated by commas. If the source has an identified non-X-ray counterpart (see bytes 101-155 below) the first name in this field is the discovery designation. if this field contains a non-X-ray designation, but the source is not assigned a counterpart in bytes 101-155, then the identification is not regarded by Dolan as well-established. --- Note Note in notes file. This number refers to the notes file, described in notes.dat below. The notes contain references and additional explanation. --- RA1 Right Ascension (B1950) in sexagesimal units Right ascension in hours, minutes and seconds, with colons (:) separating the units. The seconds, or the minutes and the seconds are often omitted. The least significant units may have a decimal fraction. --- DEC1 Declination (equinox 1950) Declination in degrees, arc minutes, and arc seconds, with colons (:) separating the units. The seconds, or the minutes and the seconds are often omitted. The least significant units may have a decimal fraction. --- RAdeg Right ascension (B1950) in degrees deg DEdeg Declination in degrees (equinox 1950) deg GLON Galactic longitude, l(II), degrees Galactic coordinates, calculated from the equatorial coordinates given in bytes 47-69. deg GLAT Galactic latitude, b(II), degrees deg Uflux 4U (2-6) kev flux, or in 10-11 ergs cm-2s-1 Data on objects with identified optical counterparts. The number of such objects is 346. 10fW/m2 Osrc Name of optical counterpart --- V Magnitude of counterpart, V (see below) mag MagType Type of magnitude Type of magnitude: * = B magnitude (otherwise the magnitude is V) V = variable star --- ObjType Type of object Two codes may be present, separated by a plus sign. The contents of this field are left justified. A = globular cluster C = cluster of galaxies G = galaxy H = HII region P = pulsar Q = quasi-stellar object R = supernova remnant S = stellar T = transient (nova-like optically) --- RA2 Right ascension, (1950) see bytes 47-57 In some cases a second set of coordinates may be present. They are equatorial coordinates, equinox 1950. They positions used to calculate galactic coordinates are the first set. --- DEC2 Declination, (1950) see bytes 59-69 --- Notes Num Note number This number is referred to in the flag in bytes 43-45 of data.dat of this catalogue. A note may take up more than one record. If so, all the records have the note number. --- flag ':' if this is the first record of a note --- note Text of note --- C.-H. Joseph Lyu Hughes STX/NASA 1997 Jan 14 The original ADC documentation by Robert S. Hill (1984) was used to create this ReadMe file. UNKNOWN UNKNOWN The Catalogue of X-Ray Positions was received from J.F. Dolan in June, 1983, as two machine-readable files of card images. The Astronomical Almanac list was selected from a subset which contains only sources with identified counterparts. For the present version, text editor line numbers were removed; the format of the notes was simplified; in-line documentation was removed (and used in this document); multiple data records for individual objects were combined into larger single records; galactic coordinates were calculated; the decimal degree equatorial coordinates were recomputed; redundant information, present in both of the component files, was edited to appear only once. The work on this catalogue revealed an erratum on page H65 of the Astronomical Almanac for 1984. G65.2 + 6.7 should be G65.2 + 5.7 (R.A. 19h 32m). VII_55.xml A Table of redshifts for Abell Clusters 7056 VII/56 Redshifts for Abell Clusters A Table of redshifts for Abell Clusters C L Sarazin H J Rood M F Struble Astron. Astrophys. 108, L7 ??? ??? 1982 1982A&A...108L...7S VII/110 : Abell et al. (1989ApJS...70....1A) "Catalogue of rich clusters of galaxies" VII/165 : Andernach H., 1991 "Compilation of published redshifts for ACO galaxy clusters" VII/177 : Struble M.F. and Rood H.J. (1991ApJS...77..363S) "Compilation of redshifts and velocity dispersions for Abell clusters" J/ApJ/365/66 : Huchra et al. (1990ApJ...365...66H) "A deep Abell cluster redshift survey" A - weighted average of HGT and HSM. B - weighted average of HGT and N. C - Corwin, H.G. Jr. 1974, Astron. J. 79, 1356. Cea - Cooke, J.A., Emerson, D., Kelly, B.D., MacGillivray, H.T., and Dodd, R.J. 1981, Monthly Notices Roy. Astron. Soc. 196, 397. D - Dressler A. 1980, Astrophys. J. Suppl. 42, 565. E - weighted average of Hea and MQa. F - average of HGT and N. Gea - Gioia, I.M., Geller, M.J., Huchra, J.P., Maccacaro, T., Steiner, J.E., and Stocke, J. 1982, Astrophys. J. 255, L17. HGT - Hoessel, J.G., Gunn, J.E., and Thuan, T.X. 1980, Astrophys. J. 241, 486. Hea - Hill, J.M., Angel, J.R.P., Scott, J.S., Lindley, D., and Hintzen, P. 1980, Astrophys. J. 242, L69. HSM - Hintzen, P., Scott, J.S., and McKee, J.D. 1980, Astrophys. J. 242, 857. KUC - Kowalski, M.P., Ulmer, M.P., and Cruddace, R.G. 1982, preprint. Mea - Mason, K.O., Spinrad, H., Bowyer, S., Reichert, G., and Stauffer, J. 1981, Astron. J. 86, 803. MQa - Melnick, J., and Quintana, H. 1981a, Astron. Astrophys. Suppl. 44, 87. MQb - Melnick, J., and Quintana, H. 1981b, Astron. J. 86, 1567. N - Noonan, T.W. 1981, Astrophys. J. Suppl. 45, 613. PL - Perrenod, S.C., and Lesser, M.P. 1980, Pub. Astron. Soc. Pac. 92, 764. Rea - Reichert, G., Mason, K.O., Lea, S.M., Charles, P.A., Bowyer, S., and Pravdo, S. 1981, Astrophys. J. 247, 803. SRa - Struble, M.F., and Rood, H.J. 1982a, Astron. J. 87, 7. SRb - Struble, M.F., and Rood, H.J. 1982b, preprint. Redshifts Clusters, galaxy The catalog gives redshifts for 329 Abell clusters, all those known to the authors in published or preprint form at the time of the compilation (through 1982). The data table has been compiled critically, based partially on a number of photometric distance estimators derived from the redshift data. These were used to evaluate probable accuracies of the redshifts and to resolve discrepancies among different values for the same clusters. The catalog includes Abell (1958) cluster numbers, redshifts, and the number of redshifts of different galaxies averaged to determine the cluster value. The machine version was prepared at the Astronomical Data Center, NASA/GSFC. Note that Struble and Rood published further compilations in 1987 (1987ApJS...63..543S) and 1991 (1991ApJS...77..363S). Other redshift compilations are also available in electronic form (see "See also" section below).
Redshift values Abell Abell cluster number (Catalog <VII/110>) --- n_Abell * when a note exists in file "notes.dat" --- z The redshift number=1 the precision varies and is based on the estimated accuracy of the determination. When values are given to fewer than four decimal places, the remaining bytes are blank. --- o_z Number of redshifts of different galaxies averaged --- r_z Reference code for the source of the determination (see below) --- Notes to individual clusters Abell Abell cluster number. --- Seq Integer used to sequentially number remarks for the same cluster. --- Text Remarks in upper and lower case characters. --- Gail L. Schneider SSDOO/ADC Francois Ochsenbein CDS 1995 Dec 15 Appreciation is extended to the authors for permission to make these data machine-readable and to distribute the catalog to the astronomical community. They have also reviewed the document prior to final printing. UNKNOWN UNKNOWN * November 1983 (Wayne H. Warren Jr., NSSDC/WDC-A-R&S 83-18): The data and notes files of A Table of Redshifts for Abell Clusters were created at the Astronomical Data Center by keying the data directly to a computer disk. The data were listed, checked against the source reference, and transferred to magnetic tape. * December 1995: Documentation standardized at CDS (Francois Ochsenbein) VII_56.xml List of Globules Based on 7 Lists by Wesselius 7057 VII/57 List of Globules List of Globules Based on 7 Lists by Wesselius P R Wesselius private communication ??? ??? 1979 1979 Interstellar dust Wesselius compiled this list based on seven lists. The main list is one in preparation in Australia supplied by Miller Goss, a second list obtained from Bok that he referred to as the Catalog of Southern Globules, Hartley-Manchester Catalog (1978), and five other lists from Bok and Cordwell (1973), Martin and Barrett (1978), Bok, Cordwell, and MacCarthy (1974), and Sim (1968a, 1968b). Wesselius notes that this list is not complete in any sense. The fields in the catalog are: running number (1-821), name of globule, B1950.0 positions, position in galactic coordinates, approximate angular size, and reference.
List of Globules ID Sequential number of record (from 1- 821) --- Name Name of globule. Wesselius' globules list was based on 7 lists: The main list is one prepared in Australia. He originally got a preliminary printout of Miller Goss (Ref. 1). In end 1978 a list that Bok had in his possession while visiting Groningen (Ref. 2). Wesselius referred to it as: the Catalog of Southern Globules, Hartley-Manchester Catalog; this version was presented to Bok in October 1978 as a computer printout. The other lists used were: 3. Bok, B. J.,Cordwell, C.S.;1973; "Molecules in the Galactic Environment", edited by M.A. Gordon and E. Snyder (New York; John Wiley and Sons Inc.), p. 82-86. 4. Martin, R.W., Barrett, A.H.;1978, Ap.J. Suppl. 36, p. 4. 5. Bok, B.J., Cordwell MacCarthy, C.; 1974, Astron. J.79, 43. 6. Sim, M. E.; 1968, Publications of the Royal Observatory, Edinburgh, Vol.6, No.8, p. 191-194. 7. Idem as 6, p. 196-198. This list of globules was not complete. For the southern sky a preliminary list concerning part of the sky was used. For the northern sky the only overall list available was that of B.T. Lynds of dark nebulae, but this covers in general larger dark regions than globules, and was not incorporated in the list (Wesselius, private communication). --- RAh Right ascension (equinox B1950.0) in hours h RAm RA in minutes min RAs RA in seconds s DE- Sign of Declination (equinox B1950.0) --- DEd DEC in degrees deg DEm DEC in arc minutes arcmin DEs DEC in arc seconds arcsec GLON Galactic longitude l(II) deg GLAT Galactic latitude b(II) deg SizeRA Approximate size in right ascension Approximate angular size (this field is blank in 20 records) arcmin SizeDEC Approximate size in declination arcmin ref Reference For the numbered list of references, see bytes 6-19 above. --- C.-H. Joseph Lyu Hughes STX/NASA 1997 Jan 14 The original ADC documentation by Robert S. Hill and Theresa A. Nagy (1981) was used to create this ReadMe file. UNKNOWN UNKNOWN This catalogue was received at NASA/Goddard Space Flight Center (GSFC) on magnetic tape from P. R. Wesselius, Laboratorium voor Ruimteonderzoek, Rijksuniversiteit, Groningen, The Netherlands, in February 1980. The data given were not edited or altered at GSFC, but the following information was added: sequential number of record (bytes 1-4) new galactic coordinates (bytes 38-52) The logical record length was decreased from 80 bytes to 66 bytes through the removal of blanks. For references, see bytes 6-19. VII_57.xml Near-Infrared Source Counts in the Galactic Plane 7060 VII/60 Near-Infrared Source Counts in the Galactic Plane Near-Infrared Source Counts in the Galactic Plane K Kawara T Kozasa S Sato H Okuda Y Kobayashi J Jugaku Mem. Fac. Sci., Kyoto Univ., Ser. A 36 353 1983 1983KyoMe..36..353K Galactic plane Photometry, infrared Infrared sources This catalog is a list of 1,989 sources detected along the galactic plane between longitudes 349 and 45 degrees. The total scanned area was 12 square degrees and all sources brighter than magnitude 6.5 in the K band are listed. The observations were made during 1978 and 1979 using a specially designed multicolor photometer. The sources are listed in ascending order in right ascension, separately for the 17 fields from l=349 deg to l=45 deg. The estimated rms position errors range from 15" to 20" in both declination and right ascension, after correcting for systematic errors (Kawara et al. 1983).
Multicolor photometric data GLON Galactic longitude, l(II) deg GLAT Galactic latitude, b(II) deg RAh Right ascension (degrees) B1950.0 h RAm RA in minutes min RAs RA in seconds s DE- Sign of Declination --- DEd Declination (degrees) B1950.0 deg DEm Dec in arcminutes arcmin DEs Dec in arcseconds arcsec Imag I magnitude mag Hmag H magnitude mag Kmag K magnitude mag Lmag L magnitude mag HKcolor H-K color mag C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 30 The original ADC documentation by Wayne H. Warren (1992) was used to create this ReadMe file. UNKNOWN UNKNOWN The data were supplied to the Astronomical Data Center, NASA Goddard Space Flight Center, as a series of 17 files on magnetic tape, by Dr. K. Kawara. The 17 files, representing the individual areas scanned, were moved to disk storage, concatenated to a single file, and reformatted to minimize storage. The sources were then sorted by increasing galactic longitude. The magnitudes in the I, H, K, and L bands are given. The fluxes for a zero-magnitude star (um = micrometers) are defined as: I (0.82 um) - 1.08 x 10**-12 W/cm**2/um H (1.61 um) - 1.20 x 10**-12 W/cm**2/um K (2.21 um) - 3.8 x 10**-12 W/cm**2/um L (3.58 um) - 6.8 x 10**-12 W/cm**2/um The H-K colors are given only for sources of H magnitude 6.5 and brighter. Data format modified at the Astronomical Data Center (ADC)/NASA GSFC, 1992 January. VII_60.xml Morphological Catalog of Galaxies (MCG) 7062A VII/62A Morphological Cat. of Gal. Morphological Catalog of Galaxies (MCG) B A Vorontsov-Velyaminov A A Krasnogorskaya Part I +90 to +45deg Trudy Gosud. Astron. Inst. Sternberg 32 ??? ??? 1962 1962TrSht..32....1V Morphological Catalog of Galaxies (MCG) B A Vorontsov-Velyaminov V P Arkhipova Part II +45 to +15 deg Trudy Gosud. Astron. Inst. Sternberg 34 ??? ??? 1964 1964TrSht..34....1V Morphological Catalog of Galaxies (MCG) B A Vorontsov-Velyaminov V P Arkhipova Part III +15 to -09 deg Trudy Gosud. Astron. Inst. Sternberg 33 ??? ??? 1963 1963TrSht..33....1V Morphological Catalog of Galaxies (MCG) B A Vorontsov-Velyaminov V P Arkhipova Part IV -09 to -33 deg Trudy Gosud. Astron. Inst. Sternberg 38 ??? ??? 1968 1968TrSht..38....1V VII/100 : contains the Part V (declination -33 to -45deg, published as Trudy Gosud. Astron. Inst. Sternberg 46, 1974) Dreyer, J.L.E. 1888, "New General Catalogue of Nebulae and Clusters of Stars", MmRAS Soc. 49, Part I (London: Royal Astronomical Society 1962, reprinted) Dreyer, J.L.E. 1895, "Index Catalogue of Nebulae found in the Years 1888- 1894, with Notes and Corrections to the New General Catalogue", MmRAS Soc. 51, 185 (London: Royal Astronomical Society 1962, reprinted) Dreyer, J.L.E. 1908,"Second Index Catalogue of Nebulae and Clusters of Stars, containing Objects found in the years 1895-1907, with Notes and Corrections to the New General Catalogue and to the Index Catalogue for 1888-1894", MmRAS Soc. 59, Part 2, 105 (London: Royal Astronomical Society 1962, reprinted) Galaxy catalogs The catalog is a compilation of information for approximately 34000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29000 galaxies and information on the remaining 5000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones, counting from the equator, and is numbered from +15 (corresponding to +90 deg) to +01 (+06 zone) and +00 (equatorial zone) to -05 (-30 zone); the fields are numbered with increasing right ascension. The catalog includes cross-identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for B1950.0, magnitudes, estimated sizes and intensities of the brighter inner region and the entire object, and estimated inclinations.
The MCG Catalogue, Vols 1-4 MCG Morphological Catalog of Galaxies (MCG) number --- n_MCG '*' if there is a note in the published version --- OtherName Catalog number in the NGC or IC --- RAh Hours RA, equinox 1950.0 h RAm Minutes RA, equinox 1950.0 min DE- Sign Dec, equinox 1950.0 --- DEd Degrees Dec, equinox 1950.0 deg DEm Minutes Dec, equinox 1950.0 arcmin Mag Photographic Magnitude mag MajAxisIn Diameter of the major axis, bright inner part arcmin MinAxisIn Diameter of the minor axis, bright inner part arcmin MajAxis Diameter of major axis, entire galaxy arcmin MinAxis Diameter of minor axis, entire galaxy arcmin IntIn [1/6] Intensity of inner region of the galaxy from 1 (completely black image) to 6 (image barely visible). --- IntOut Intensity of outer region of the galaxy --- Incl Inclination of the principle Plane from 1 (face on) to 5 (edge on). '?'= uncertainty. --- adc.doc Documentation by Wayne H. Warren Jr. Francois Ochsenbein CDS 1994 Nov 18 UNKNOWN UNKNOWN * 18-Nov-1994: Compared to the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory "nonstell/galaxies/mcg", the following errors have been corrected: - Misalignments in records 6734 10857 13382 25010 - Errors in the "Incl" parameter for records 3601(MCG+09-11-008) 4053(MCG+09-16-022) 6928(MCG+08-30-002) 13323(MCG+04-06-049) - Error in "MajorAxis" parameter for record 19653(MCG+01-37-012) * 22-Oct-1996: Gail L. Schneider (SSDOO/ADC) - Error in "MCG" for record 4341 corrected For: MCI+09-19-067 Read: MCG+09-19-067 VII_62A.xml Catalog of CO Observations of Galaxies 7064 VII/64 CO Observations of Galaxies Catalog of CO Observations of Galaxies F Verter ApJS 57 261 1985 1985ApJS...57..261V VII/139 : CO Observations of Galaxies 1985-1989 (Verter 1990) Bottinelli, L., Gouguenheim, L., and Paturel, G. 1983, General Catalog of 21 cm Line Data, unpublished. de Vaucouleurs, G., de Vaucouleurs, A., and Corwin, H. G., Jr. 1976, Second Reference Catalogue of Bright Galaxies (Austin: University of Texas Press). Fisher, J. R., and Tully, R. B. 1975, Astr. Ap., 44, 151. Morris, M., and Rickard, L. J. 1982, Ann. Rev. Astr. Ap., 20, 517. Rood, H. 1980, A Catalog of Galaxy Redshifts, unpublished. Sandage, A., and Tammann, G. A. 1981, A Revised Shapley-Ames Catalog of Bright Galaxies (Washington, DC: Carnegie Institution of Washington). Ulrich, B. L., and Haas, R. W. 1976, Ap. J. Suppl., 30, 247. Verter, F. 1985, Ap. J. Suppl., 57, 261. Bibliography Carbon monoxide Galaxy catalogs References The catalog is a complete summary of all observations of CO isotopes in galaxies up to spring 1984. It consists of seven tables. Refs.dat describes the reference for CO observations of galaxies. Telescop.dat describes the properties of the telescopes used for observations. Detect.dat and uprlmits.dat contain a compilation of data on galaxies that have been observed in CO. Most of the characteristics listed here are observed properties. The detected galaxies are listed first, followed by galaxies with upper limits. Upper limits are given for detected galaxies if the detection is disputed or if the limits refer to transitions or regions that have not yet been detected. Temp.dat is a comparison of the antenna temperature scales used in the references in this catalog. Maps.dat lists the coverage, resolution, observed structure of CO maps of galaxies, and notes.dat contains notes to tables.
References Code Code name Character string that represents the reference in the following files. If this field is blank, the reference, description, telescope, and features: fields are continuations of the previous record. --- Ref Reference --- Desc Brief description of the paper --- Telesco Telescope Standard abbreviation for the telescope that made the observations; see Telescopes (telescop.dat). --- Feature Features Describes the features observed. The following abbreviations were used: nuc - galaxy nuclei dust - patches of obscuration H II - H II regions OB - OB associations M - there is a map A map is defined as three or more detected positions per galaxy; see CO Maps of Galaxies (maps.dat). --- Telescopes Telesco Telescope Standard abbreviation for the observing facility. --- Diam Diameter m FWHM Beam FWHM Full width at half maximum in minutes of arc. arcmin Freq Frequency Observing frequency of beam FWHM in GHz. GHz Ref Reference Literature reference for equipment and performance of the telescope. This can either be a code name (see refs.dat, or a complete reference. --- Detections ID Galaxy name Galaxies with NGC numbers are listed first, followed by IC, DDO, Mk, and named galaxies. Alternate names are given if they are one of the above, or a Messier number. --- RMType Revised morphological type Revised morphological type from the Second Reference Catalogue of Bright Galaxies (de Vaucouleurs, de Vaucouleurs, and Corwin 1976; RC2). --- MType Morphological type Morphological type from the Revised Shapley-Ames Catalog (Sandage and Tammann 1981; RSA). --- MaxisD Major axis diameter The apparent major axis diameter of the galaxy, measured at the 25 mag sq. arcsec surface brightness isophote. The diameters are from the RC2 in units of minutes of arc. arcmin Nflag1 Note flag Lowercase letter that corresponds to the note flag described in Notes to CO Observations (notes.dat). All of the note flag fields appearing below are defined similarly. --- BlueMag Apparent blue magnitude The apparent blue magnitude of the galaxy in the B(T) system of RC2. The numbers quoted were taken from the RSA, and have been corrected for galactic and internal absorption. The absorption corrections are described in the RSA. Since blue magnitudes were not available for the DDO galaxies, apparent photographic magnitudes from the Fisher and Tully (1975) survey of the DDO list are given for these objects. These magnitudes are not corrected for galactic or internal absorption. mag Nflag2 Note flag --- RV Radial velocity Radial velocity, in units of km/sec of the galaxy relative to the center of the Local Group. The velocities are taken from the unpublished Catalog of Galaxy Redshifts (Rood 1980), which is available on magnetic tape from the ADC. km/s Nflag3 Note flag --- Cflag Component flag For one galaxy (IC 4553), this field will contain an N, meaning the radial velocity is for the northern component, or an S for the southern component. --- HIflux H I flux Total H I flux of the galaxy, in units of Jy*km/sec. The fluxes are taken from the unpublished General Catalogue of 21 Centimeter Line Data (Bottinelli, Gouguenheim, and Paturel 1983; BGP). The BGP does not include DDO galaxies, so H I fluxes are taken from the Fisher and Tully (1975) survey of the DDO catalog. The format of the field is as follows: Mantissa bytes 66-69, format F4.1 Left parenthesis byte 70, format A1 or 1X Exponent byte 71, format I1 Right parenthesis byte 72, format A1 or 1X Note flag byte 73, format A1 Jy/km/s LeftP1 Left parenthesis --- Exp1 Exponent --- RightP1 Right parenthesis --- Nflag4 Note flag --- VelWidth H I FWHM The full velocity width of the H I profile, defined so that 50% of the profile area falls within this width. For the BGP galaxies, these widths were all remeasured on the original profiles and therefore constitute a homogeneous sample. --- Nflag5 Note flag --- Mflag Mapping flag If the character M appears in this byte, the galaxy has been mapped and the other parts of the sampling field will be blank. --- Sampling Sampling The sampling of the CO observations, defined as the fraction of the optical galaxy that was surveyed. The sampling is given as the product of the resolution of the observations times the number of positions in the galaxy that were examined. Note on Resolution - the fraction of the optical galaxy covered by a single telescope beam. --- LeftP2 Left parenthesis --- Exp2 Exponent --- RightP2 Right parenthesis --- ObsNum Number of observations --- TempCom Temperature comment character < - upper limit ? - marginal detection N - not available P - in preparation --- AntTemp Peak antenna temperature Peak antenna temperature of the detected galaxy. The format of the field is as follows. --- COcode CO transition code blank - J=1-0 transition of 12CO (2-1) - J=2-1 transition of 12CO (13) - J=1-0 transition of 13CO (18) - J=1-0 transition of C18O --- EmisCom Emission comment character Character N, for not available, if the published detection was presented only as an antenna temperature. --- TotEmis Total observed emission The total observed integrated emission ... for detected galaxies. For most mapped galaxies the total emission is not published and cannot easily be deduced from the data in the literature. Hence, this field primarily lists the integrated emission of galaxies detected at a single point ... that can be inferred from the features field of refs.dat above. K/km/s COflux Extrapolated net CO flux The extrapolated total CO flux that represents the entire emission of a detected galaxy. See Verter (1985) for a discussion of how these values were obtained. Jy/km/s LeftP3 Left parenthesis --- Exp3 Exponent --- RightP3 Right parenthesis --- Ref Reference code, see Reference (refs.dat) --- Upper Limits ID Galaxy name --- MType Morphological type --- MaxisD Major axis diameter arcmin Nflag1 Note flag --- BlueMag Blue magnitude mag Nflag2 Note flag --- RV Radial velocity km/s Nfalg3 Note flag --- Cflag Component flag --- HIflux H I flux Jy/km/s LeftP1 Left parenthesis --- Exp1 Exponent --- RightP1 Right parenthesis --- Nflag4 Note flag --- VelWidth H I FWHM --- Nflag5 Note flag --- Sampling Sampling --- LeftP2 Left parenthesis --- Exp2 Exponent --- RightP2 Right parenthesis --- ObsNum Number of observations --- TempCom Temperature comment character --- NAntTemp Noise antenna temperature Noise antenna temperature of a galaxy with upper limits. When a reference contained upper limits for several points in a galaxy, the average is shown. The significance level of the upper limits, defined as the factor by which the rms noise temperature of the reported null detections has been multiplied, is listed for each reference in temperatures.dat The format of the field is as follows: Note on Comment char < - upper limit N - not available P - in preparation --- Ref Reference code --- Temperatures Ref Reference code See References (refs.dat). If this field is blank, the corrections and comments fields are continuations of the previous record. --- Telesco Telescopes. See telescop.dat --- Siglevel Significance of upper limits The significance level of the upper limits given in the reference, defined as the factor by which the rms noise temperature of the reported null detections has been multiplied ... Upper limits at the same significance level may still represent different sensitivities if the data differ in velocity resolution. If this byte is blank, the reference did not have any upper limits. --- Avaflag Availability flag If this byte contains a question mark, the significance level was not given in the reference. --- Nflag Note flag Lowercase letter that corresponds to the note flag described in Notes to CO Observations (notes.dat). --- TempS Temperature symbol The symbol which was used in the reference for the final temperature scale. Different authors have used different approaches to obtain temperatures labeled T(A) --- Correc Corrections Antenna efficiency corrections described in the reference. --- note Comments A UH in this field indicates that the reference claims to have employed the chopper wheel calibration technique described in Ulrich and Haas (1976). --- CO Maps of galaxies ID Galaxy name If this field is blank, the resolution, number of map points, shape of points, and reference fields are continuations of the previous record. --- Dtype Distribution type The structure of the observed CO distribution, according to the classification scheme of Morris and Rickard (1982). In this scheme, the distribution types are distinguished by the strength of the central source and the degree of continuity of the disk emission, as follows: 1 - central source + disk 2 - central source + annulus 3 - annulus without central source 4 - emission from isolated regions 5 - no detectable emission (not used in this file) --- Nflag1 Note flag Lowercase letter that corresponds to the note flag described in Notes to CO Observations (notes.dat). All of the note flag fields appearing below are defined similarly. --- IncAng Inclination angle deg Nflag2 Note flag --- Res Resolution The resolution of the observations, defined in the sampling field of detections.dat as the FWHM area of the antenna beam divided by the area inside the 25 mag/sq arcsec. surface brightness isophote of the galaxy. The isophotal areas were calculated using the diameters given in RC2 and the inclination angle ... As defined, the colloquial expression high resolution corresponds to low numbers in this field. --- LeftP Left parenthesis --- Exp Exponent --- RightP Right parenthesis --- Nflag3 Note flag --- NumMap Number of map positions observed --- Spts Shape of points Describes the location and grouping of the observed positions. A line is a string of points that goes through the center of the galaxy, and is often aligned with the major axis (MA) or minor axis (mA). A cross is two lines at roughly right angles, whereas a strip is a line that does not pass through the center. When many positions at more or less even spacings are observed, the map points are a grid. --- Ref Reference See References (refs.dat). --- Notes Fflag File flag D if the note is from detect.dat or uprlmits.dat; T if the note is from temp.dat; or M if the note is from CO Maps of Galaxies (maps.dat). --- Nflag Note flag Lowercase letter that corresponds to a note flag from any of the files listed above. If this byte is blank, the note text is a continuation of the previous record. --- Ntext Note text --- C.-H. Joseph Lyu Hughes STX/NASA Gail L. Schneider SSDOO 1996 Feb 28 UNKNOWN UNKNOWN The original ADC documentation by Lee E. Brotzman was used to create this ReadMe file. The Catalog of CO Observations of Galaxies was sent to the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, by the Centre de Donnees Stellaires (CDS) in January 1985. This version was in the form of a typesetting input tape as used to produce the published paper. The original tape contained six files: a file with the text of the published paper and one file for each of the tables in the paper. The table files contained column headings, spacing control information, and the notes. ADC personnel made a separate file for the notes, removed all column headings and blank records, and reduced each column to a common format. A FORTRAN program was run that checked the validity of each field according to its data type and value. The only file not included in the version of the VCO distributed by the ADC is the file containing the text of the published paper. VII_64.xml Catalogue of Dark Nebulae and Globules for Galactic Longitudes 240 to 360 degrees. 7068A VII/68A Dark Nebulae and Globules for l=240-360deg Catalogue of Dark Nebulae and Globules for Galactic Longitudes 240 to 360 degrees. J V Feitzinger J A Stuewe Astron. Astrophys. Suppl. Ser. 58 365 1984 1984A&AS...58..365F Catalogue of Dark Nebulae and Globules for Galactic Longitudes 240 to 360 degrees. J V Feitzinger J A Stuewe Astron. Astrophys. Suppl. Ser. 63 203 1986 1986A&AS...63..203F Globules Nebulae (adapted from Anne C. Raugh, NASA STI-T-1-5810-508-86) The catalog is a compilation of data gleened from a study of the European Southern Observatory Quick Blue Survey (ESO(b)) and SRC-J Sky Atlas on 489 dark clouds and 331 globules. The data compiled include position, size, opacity and morphological classification (in the system of van den Bergh, 1972). Also included is a FITS file containing a 500x1400 pixel map of the survey area.
The Dark Clouds The Globules FEST Running Number --- Field Field number in ESO/SRC Survey --- Foil Foil (SRC) or Plate (ESO) number=1 In general, the SRC-J foils were the primary source of data and the corresponding ESO(B) glass plates were used as a validity check. When the foil was not available the plate became the primary source. "ESO" indicates the data were taken from the ESO(B) glass plate of the survey field. "SRC" indicates the data were taken from the SRC-J foil of the survey field. --- Seq Number in field number=2 Generally this is an integer, but in two cases (both globular filaments) this is a Roman numeral, right-justified within the character field. --- Desc Two-letter code description number=3 the two-letter code describing the appearance of the object: CG Cometary globule DC Dark cloud DF Dark filament EN Embedded in (bright) nebulosity GF Globular filament ST Worm track or elephant trunk (equivalent to WT) TA Tail of a cometary globule WT Worm track or elephant trunk (equivalent to ST) --- GLON Galactic longitude of center deg GLAT Galactic latitude of center deg RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Area Area (for dark nebulae) deg2 Mult Number of globules ("globules" file) number=8 if the object is actually a complex of globules, Mult is the number of individual globules. The coordinates given refer to the approximate center of the entire complex. --- OpClass Opacity class number=4 Opacity on a scale of 1 to 6, 6 being the most opaque. --- Class van den Bergh Classification number=5 van den Bergh classification scheme consists of four different classes, each denoted by a single Greek letter: ALPHA Amorphous cloud exhibiting very fuzzy or indistinct edges BETA Clouds with some structure and relatively well-defined edges GAMMA Absorption features with sharp edges which are not located in H II regions DELTA Sharp-edged absorption features located in H II regions For objects that fall between classes, the Greek letters are abbreviated as A B G D respectively. For some cometary globules the head and tail have distinct opacities and van den Bergh classifications. --- i Galactic inclination angle number=6 Inclination angle of elongated dark clouds measured counterclockwise against the galactic plane,:eq. in degrees. deg Xmm X-plate coordinate mm Ymm Y-plate coordinate mm Ident Cross-references number=7 Cross references consist in two-letter code followed by an up to three-digit number that identifies the object as also being listed in the reference denoted by the letter code. SL Sandqvist and Lindroos S Sandqvist (1977) CG Zealy et al. (1983) The numbers are those of the object in the cited paper. In some cases the object appeared in more than one paper, in which case there are two or more full references, or appears more than once in a single paper, in which case the additional numbers are separated by commas (for example, the cross-reference for dark nebula number 225 is S 155,157) --- skymap.fit FITS Map of survey area Anne C. Raugh ADC Francois Ochsenbein CDS 1995 Jun 13 UNKNOWN UNKNOWN * 1986 (Anne C. Raugh, ADC): The catalogue was sent to the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, by the Centre de Donnees Astronomiques (CDS), in February 1986. The original tape contained four text files formatted in the same manner as in the published catalog. The catalog was so well formatted that the only editing done was to correct several minor typographic errors and to replace the character string "---" indicating a null value for the inclination field, with a string of blanks, in order to avoid errors in trying to read that field with a FORTRAN I5 format. A FORTRAN program was run that checked the validity of each field according to its data type and value. * 13-Jun-1995: standardised at CDS, and homogenized the formats of the two files "darkneb" and "globules" such that they share the same "Byte-by-Byte description" VII_68A.xml The Asiago Catalogue of Quasi-Stellar Objects 7069 VII/69 Asiago Catalogue of QSOs The Asiago Catalogue of Quasi-Stellar Objects C Barbieri M Capaccioli S Custiani G Nardo A Omizzolo Mem S.A. It. 54 3 601 1983 1983MmSAI..54..601B VII/158 : Catalog of Quasi-Stellar Objects (Hewitt & Burbidge 1993) VII/188 : Quasars and Active Galactic Nuclei (7th Ed.) (Veron+ 1996) QSOs Redshifts The Asiago Catalog of 2004 Quasi Stellar Objects (QSOs) is an updated version of that published by Barbieri, Capaccioli and Zambon in 1975 (1975MmSAI..46..461B). Most of the information of these objects are taken from the literature published before Dec. 31, 1981. Specifically, the catalog.dat file contains names, equatorial and galactic coordinates, photometry, redshifts, information on radio emission, variability, morphology, presence of absorption lines, for 2004 QSOs. The indexed references (in refs.dat) and further detailed information (in remarks.dat) concerning absorption spectra, X-ray properties, and cross-reference tables are also provided.
The Catalogue Name QSO name --- u_Vmag The '-' means uncertain photometry --- Vmag Visual magnitude mag B-V (B-V) color mag U-B (U-B) color mag r_Vmag Reference for photometry --- u_z The '-' means uncertain redshift --- z Redshift, normally from emission line --- r_z References of redshift (more in remarks) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec r_DEd Reference of position --- NoteSum SumNote number=1 the NoteSum and u_NoteSum codes are made by summing up the numbers corresponding to the following notes: 01: radio quiet 02: radio variability 04: optical variability 08: nebulosity or jet 16: absorption lines 32: spectral variability (examples: NoteSum = 17 means: radio quiet with absorption lines; NoteSum=04 and u_NoteSum=04 means: uncertain optical variability ) --- u_NoteSum Uncertainties on SumNote number=1 the NoteSum and u_NoteSum codes are made by summing up the numbers corresponding to the following notes: 01: radio quiet 02: radio variability 04: optical variability 08: nebulosity or jet 16: absorption lines 32: spectral variability (examples: NoteSum = 17 means: radio quiet with absorption lines; NoteSum=04 and u_NoteSum=04 means: uncertain optical variability ) --- ExpRef Reference of deep exposure photograph showing optical structure --- ChartRef Reference to Finding Chart --- remFlag '1' for a remark in "remarks.dat" --- Remarks to individual quasars HHMM+DDd Designation based on position --- cont Continuation flag --- Text Text of remark, includes references. --- References quoted in catalog and remarks. RefNum Reference number as quoted in catalog --- Cont Continuation flag --- Text Text of reference --- Francois Ochsenbein CDS 1996 Nov 28 UNKNOWN UNKNOWN The description of this version was assumed to be identical to the previous version <VII/3> by Barbieri, Capaccioli and Zambon (1975MmSAI..46..461B) VII_69.xml Galaxies rotation curves: a catalogue. 7070A VII/70A Galaxies Rotation Curves Galaxies rotation curves: a catalogue. G C Baiesi-Pillastrini G G C Palumbo G Vettolani Astron. Astrophys. Suppl. Ser. 53 373 1983 1983A&AS...53..373B Radial velocities Galaxies, rotation Galaxy catalogs The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.
The Catalogue of Velocities Name of the Galaxy number=1 this column is repeated for measurements at several distances --- MType Morphological class of the galaxy number=1 this column is repeated for measurements at several distances --- RAh Right Ascension 1950 (hours) number=1 this column is repeated for measurements at several distances h RAm Right Ascension 1950 (minutes) number=1 this column is repeated for measurements at several distances min RAs Right Ascension 1950 (seconds) number=1 this column is repeated for measurements at several distances s DE- Declination 1950 (sign) number=1 this column is repeated for measurements at several distances --- DEd Declination 1950 (degrees) number=1 this column is repeated for measurements at several distances deg DEm Declination 1950 (minutes) number=1 this column is repeated for measurements at several distances arcmin n_RadVel A left parenthesis indicates a Heliocentric Velocity --- RadVel Radial velocity number=2 the velocity is corrected for the galactic rotation (300.sin(l).cos(b) km/s), except when n_RadVel is '(' km/s Dist Approximate extent from the center of the galaxy arcsec contour '*' when an iso-velocity contour exists --- Ref Reference --- The References Ref Reference number (assigned chronologically) --- Text Text of Reference --- Francois Ochsenbein CDS 1995 Dec 19 UNKNOWN UNKNOWN * The magnetic tape was sent in July 1985 by G.G.C Palumbo to C. Jaschek, Director of CDS (Centre de Donnees de Strasbourg, France) * From ADC: The catalogue was received by the Astronomical Data Center, NASA Goddard Space Flight Center, from the Centre de Donnees de Strasbourg (CDS), in February 1986. The original tape contained two text files formatted in the same manner as in the published catalog. An editor was used to compress the data file from 76- to 56-byte records by removing extra blank columns, as well as to make minor format changes in some name and radial velocity for uniformity. A FORTRAN program was run that checked the validity of each field according to its data type and value. As a result of running this program, it was determined that approximately 5% of the right ascensions listed were obviously in error (for example, the value given for NGC 1087 was 2 hours, 43 minutes, 86 seconds). This prompted a closer examination of all the coordinates. It was discovered that at least 15% of the right ascensions given in the catalog suffered from the same error - a right ascension of, for example, 38.3 minutes being listed as 38 minutes, 3 seconds. Several negative signs in the declination field were also missing. At that point it was decided to replace all the coordinates by equinox 1950.0 coordinates from other catalogs. The RC2 (Catalog <VII/112>) and UGC (Catalog <VII/26>) catalogs were used whenever possible. Coordinates for objects not listed in either of these were obtained from the source catalogs. During this process, two entries for VV 147 were encountered with conflicting coordinates. By comparing coordinates in the source catalog, it was determined that the first object listed was actually VV 141. The name field of that entry was changed to reflect this. An editor was also used to change the references file to upper and lower case, to add blanks, and to expand abbreviations. Several minor typographical errors were also corrected. * From CDS (December 1995): The description was standardized. A further error in the right ascension of NGC 4753 was corrected, and the references have been reformatted. VII_70A.xml Redshifts for Zwicky's Near Clusters 7071 VII/71 Redshifts for Zwicky's Near Clusters Redshifts for Zwicky's Near Clusters G C Baiesi-Pillastrini G G C Palumbo G Vettolani Astron. & Astrophys. Suppl. 56 363 1984 1984A&AS...56..363B Radial velocities Galaxies Clusters, galaxy The catalog contains a list of redshifts for Zwicky's Near Clusters. All of the 503 Zwicky Near Clusters as given in the Uppsala General Catalogue of Galaxies (UGC) are listed and radial velocity information for those that have at least one galaxy with published redshift positioned within the contours given in the Zwicky catalog is provided. Redshifts of galaxies belonging to clusters is obtained from the catalog of Radial Velocities of Galaxies. The catalog includes UGC cluster numbers, Zwicky field numbers, contour numbers, positions, heliocentric cluster radial velocities, and notes.
Catalog Data UGC UGC cluster number Number of the cluster as it is listed in the Uppsala General Catalogue of Galaxies (Nilson, 1973; UGC). The file is sorted on this field. --- Suffix Suffix Differentiates between clusters having the same UGC number. It is always either " " or "a". --- ZwickyID Zwicky catalog Identification Zwicky catalog identification. Number of the field (before hyphen) in which the cluster appears in the Zwicky catalog (Zwicky et al. 1961-68). After the hyphen one would find contour number in the Zwicky catalog. --- RAh right ascension (Equatorial Coord. 1950.0) Positions are for cluster center. h RAm RA in minutes min DE- Sign of declination (1950.0) --- DEd declination in degrees (1950.0) deg DEm DEC in arcminutes arcmin RV Radial velocity cluster/all avail. values Heliocentric radial velocity of the cluster in km/sec. Usually this is the arithmetic mean of the individual radial velocities of the galaxies in the cluster (i.e., excluding those objects apparently in the foreground or background). However, in some clusters so few galaxies had available radial velocities that the determination of a unique or even most likely cluster velocity was not possible. When this happened, all the values found were listed separately in continuation records. If all the previous fields are blank, then the data in this and the following fields are a continuation of the previous record. km/s Num Number of gal. used Number of galaxies used to determine the radial velocity given in this record. Only galaxies having published redshifts measured within the contour given in the Zwicky catalog were used in calculating this value. --- flag Note flag (see notes.dat) An asterisk (*) indicates that there is a note containing additional information about this object in the second file (notes.dat). If there is no note, this field is blank. --- Notes UGC UGC cluster number UGC cluster number of the object in the catalog file to which this note refers. The notes file is sorted on this field. --- Suffix Suffix Suffix to the UGC number to differentiate between clusters with the same UGC number: always either blank or a. If UGC and Suffix fields are blank, then the note field is a continuation from the previous record. No note requires more than one continuation line. --- note Note The text of the note. Two abbreviations are used throughout the file. They are: F : Foreground B : Background If necessary, a continuation line is used to contain the text. --- C.-H. Joseph Lyu Hughes STX/NASA 1997 Jan 27 The original ADC documentation by Anne C. Raugh (1987) was used to generate this ReadMe file. UNKNOWN UNKNOWN Redshifts for Zwicky''s Near Clusters was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in February 1986. The original tape contained two text files formatted in the same manner as the published catalog (Baiesi-Pillastrini et al. 1984). An editor was used to compress the data file from 76- to 38-byte records by removing blank columns. A FORTRAN program was run that checked the validity of each field according to its data type and value. An apparently erroneous value of declination, 63deg. 63', was found in the record for cluster number 83. A check of the UGC, source of the coordinates, revealed the same error in that catalog. Following the UGC reference, the object was located in the Catalogue of Galaxies and Clusters of Galaxies, where the declination is given as 63deg. 23'. The declination has been corrected to this value in this version of the catalog. An editor was also used to replace ditto marks with the implied words in the notes.dat file. VII_71.xml A Catalog of Stellar Velocity Dispersions. I. Compilation and Standard Galaxies 7072 VII/72 Stellar Velocity Dispersions. I. Std Galaxies A Catalog of Stellar Velocity Dispersions. I. Compilation and Standard Galaxies B C Whitmore D B McElroy J Tonry Astrophys. J. Suppl. Ser. 59 1 1985 1985ApJS...59....1W Spectroscopy Velocity dispersion A catalog of central stellar velocity dispersion measurements is presented, current through 1984. The catalog includes 1096 measurements of 725 galaxies. A set of 51 standard galaxies is defined which consists of galaxies with at least three reliable, concordant measurements.
The catalogue of adopted velocity dispersions ID Galaxy name --- MType Morphological type --- r_MType Reference of MType: * from UGC (Nilson 1973, Uppsala Ann. 6) blank from RC2 (de Vaucouleurs et al. 1976) --- VelDisp Adopted velocity dispersion km/s Source data ID Galaxy name --- MType Morphological type --- r_MType Reference of MType as above --- l_VelDisp Limit Flag on VelDisp --- VelDisp Original velocity dispersion km/s e_VelDisp Quoted mean error on VelDisp km/s ExtProf Indicator measured extd vel dispersion Indicator 1 - the authors measured extented velocity dispersion profiles 0 - the authors did not measure extended velocity disp profiles 2 - only a few measurements in the outer regions are available --- n_FWHM unit flag FWHM Indicator of unit in which FWHM is expressed: - = for 0.1nm/mm blank = for km/s --- FWHM of the narrowest comparison line (in km/s or A/mm depending on n_FWHM) --- dim1 Slit width arcsec dim2 Slit length arcsec TelSite Code related to the instrument (place and telescope) --- Det Code related to the detector and technique --- Pixels Number of pixels in spectra pix lambda1 Lower wavelength range 0.1nm lambda2 Upper wavelength range 0.1nm Source Designation of the source --- Class Numerical galaxy class (de Vaucouleurs index) --- Vel Radial velocity of the Galaxy km/s Mag Magnitude of the galaxy mag r_Mag Reference of the magnitude, as for r_MType --- Other Other designation of the galaxy --- Francois Ochsenbein CDS 1994 Paul Kuin [ADC] 13-May-1997 Jun 10 VII_72.xml IRAS Small Scale Structure Catalog 7073 VII/73 IRAS Small Scale Structure Catalog, Ver 1.00 IRAS Small Scale Structure Catalog G Helou D W Walker Jet Propulsion Laboratory ??? ??? 1985 1985isss.book.....H Photometry, infrared Nonstellar objects Infrared sources Sources resolved by the Infrared Astronomical Satellite in any band (12, 25, 60, or 100 microns) but smaller than eight arcmin in angular extent are to be found in the Small Scale Structure Catalog, also known as the catalog of "small extended sources." The catalog gives the infrared characteristics of 16740 objects including, e.g., galaxies, planetary nebulae and compact H II regions. The catalog lists for each entry and in each band separately: a position accurate to about one arcminute (rms); a flux density accurate to 50% (rms) overall, and better at high signal to noise ratios; a rough indicative size if a point source is present at the same location; and a variety of warning and processing flags. If a detailed shape description, or a more accurate poistion, flux, or size are needed, these must be determined from the raw detector output. Incompleteness is a complex function of wavelength band, brightness, and location, so the absence of an entry in the SSS Catalog does not necessarily imply the lack of detectable extended emission. Many entries, mostly at 60 and 100 microns, refer only to emission features that are details in larger structures known as Galactic cirrus. Complete documentation, including a description of the catalog format, is contained in the printed version.
IRAS Small Scale Structure Catalog Sources PSCname IRAS source name --- BMFlg Number of bands in source and band merging warning flag --- RAh Hours RA, equinox 1950.0, epoch 1983.5 h RAm Minutes RA, equinox 1950.0, epoch 1983.5 min RAs Seconds RA, equinox 1950.0, epoch 1983.5 s DE- Sign Dec, equinox 1950.0, epoch 1983.5 --- DEd Degrees Dec, equinox 1950.0, epoch 1983.5 deg DEm Minutes Dec, equinox 1950.0, epoch 1983.5 arcmin DEs Seconds Dec, equinox 1950.0, epoch 1983.5 arcsec NH_12 Number of hours-confirmed sightings, 12um --- NH_25 Number of hours-confirmed sightings, 25um --- NH_60 Number of hours-confirmed sightings, 60um --- NH_100 Number of hours-confirmed sightings, 100um --- Fnu_12 Average non-color corrected, spatially integ- rated flux density, 12um number=1 This quantity appears with a different format or representation, or is omitted in the printed version of the catalog. (2): These fields are blank if the source was not detected in the corres- ponding IRAS band. Jy Fnu_25 Average non-color corrected, spatially integ- rated flux density, 25um number=1 This quantity appears with a different format or representation, or is omitted in the printed version of the catalog. (2): These fields are blank if the source was not detected in the corres- ponding IRAS band. Jy Fnu_60 Average non-color corrected, spatially integ- rated flux density, 60um number=1 This quantity appears with a different format or representation, or is omitted in the printed version of the catalog. (2): These fields are blank if the source was not detected in the corres- ponding IRAS band. Jy Fnu_100 Average non-color corrected, spatially integ- rated flux density, 100um number=1 This quantity appears with a different format or representation, or is omitted in the printed version of the catalog. (2): These fields are blank if the source was not detected in the corres- ponding IRAS band. Jy Xtalk_12 Cross-talk flag, 12um number=1 This quantity appears with a different format or representation, or is omitted in the printed version of the catalog. (2): These fields are blank if the source was not detected in the corres- ponding IRAS band. --- Xtalk_25 Cross-talk flag, 25um number=1 This quantity appears with a different format or representation, or is omitted in the printed version of the catalog. (2): These fields are blank if the source was not detected in the corres- ponding IRAS band. --- Xtalk_60 Cross-talk flag, 60um number=1 This quantity appears with a different format or representation, or is omitted in the printed version of the catalog. (2): These fields are blank if the source was not detected in the corres- ponding IRAS band. --- Xtalk_100 Cross-talk flag, 100um number=1 This quantity appears with a different format or representation, or is omitted in the printed version of the catalog. (2): These fields are blank if the source was not detected in the corres- ponding IRAS band. --- NearPS_12 Number of near-by weeks-confirmed point sources, 12um --- NearPS_25 Number of near-by weeks-confirmed point sources, 25um --- NearPS_60 Number of near-by weeks-confirmed point sources, 60um --- NearPS_100 Number of near-by weeks-confirmed point sources, 100um --- SES1_12 Number of nearby FISES entries, 12um --- SES1_25 Number of nearby FISES entries, 25um --- SES1_60 Number of nearby FISES entries, 60um --- SES1_100 Number of nearby FISES entries, 100um --- Cir Number of hours-confirmed, 100um-only point sources --- HD High source density flag, encoded, one bit per band --- DblPS Possibility this is a double point source (1 bit per band) --- PtSrc Name of IRAS Point Source counterpart and conflict flag --- Psiz_12 Size estimate from comparison of FLUX with PTSRC flux, 12um darcsec Psiz_25 Size estimate from comparison of FLUX with PTSRC flux, 25um darcsec Psiz_60 Size estimate from comparison of FLUX with PTSRC flux, 60um darcsec Psiz_100 Size estimate from comparison of FLUX with PTSRC flux, 100um darcsec NID Number of positional associations --- IDType Type of objects associated --- Fqlt_12 12um flux quality class --- Fcat_12 12um final selection flags --- Dra_12 Right ascension offset from mean position to 12um s Ddec_12 Declination offset from mean position to 12um arcsec Unc_12 95% confidence diameter for position at 12um darcmin NS_12 Number of individual detections at 12um --- Fqlt_25 25um flux quality class --- Fcat_25 25um final selection flags --- Dra_25 Right ascension offset from mean position to 25um s Ddec_25 Declination offset from mean position to 25um arcsec Unc_25 95% confidence diameter for position at 25um darcmin NS_25 Number of individual detections at 25um --- Fqlt_60 60um flux quality class --- Fcat_60 60um final selection flags --- Dra_60 Right ascension offset from mean position to 60um s Ddec_60 Declination offset from mean position to 60um arcsec Unc_60 95% confidence diameter for position at 60um darcmin NS_60 Number of individual detections at 60um --- Fqlt_100 100um flux quality class --- Fcat_100 100um final selection flags --- Dra_100 Right ascension offset from mean position to 100um s Ddec_100 Declination offset from mean position to 100um arcsec Unc_100 95% confidence diameter for position at 100um darcmin NS_100 Number of individual detections at 100um --- Information about positional associations with sources in other catalogs PSCName IRAS source name --- RecNo Main data table record number for SSS source --- CatNum Catalog number number=1 See Table X.B.4 in the "IRAS Catalogs and Atlases Explanatory Supplement" also included in the file "meaning.txt" in this directory. --- Source Source identification --- Type Source type or spectral class --- Radius Radius vector from IRAS source to association arcsec Pos Position angle (E of N), IRAS source to object deg Field1 Object data field 1, catalog dependent number=1 See Table X.B.4 in the "IRAS Catalogs and Atlases Explanatory Supplement" also included in the file "meaning.txt" in this directory. --- Field2 Object data field 2, catalog dependent number=1 See Table X.B.4 in the "IRAS Catalogs and Atlases Explanatory Supplement" also included in the file "meaning.txt" in this directory. --- Field3 Object data field 3, catalog dependent number=1 See Table X.B.4 in the "IRAS Catalogs and Atlases Explanatory Supplement" also included in the file "meaning.txt" in this directory. --- irassss.doc The original ADC document meaning.txt Details of association catalogues Gail L. Schneider SSDOO/ADC 1998 Apr 08 VII_73.xml Atlas of Peculiar Galaxies 7074A VII/74A Atlas of Peculiar Galaxies Atlas of Peculiar Galaxies H C Arp Astrophys. J. Suppl. Ser. 14 1 1966 1966ApJS...14....1A VII/170 : "Catalogue of Southern Peculiar Galaxies and Associations", by Arp H.C. and Madore B.F., 1987, Cambridge Univ. Press VII/192 : Arp's Peculiar Galaxies (Webb 1996) 1: Humason M.L., Mayall N.U., Sandage A.R., =1956AJ.....61...97H 4: de Vaucouleurs G., de Vaucouleurs A., 1964, Ref. Cat. of Bright Galaxies (Univ. Texas Press, Austin) (RC1) Vorontsov-Velyaminov B.A., Arkhipova V.P., 1964 "Morphological Catalogue of Galaxies", Moscow <CDS Catalogue: VII/62A> 13: Burbidge E.M., Burbidge G.R., =1959ApJ...130...15B 22: Burbidge E.M., Burbidge G.R., =1964ApJ...140.1307B 23: Burbidge E.M., Burbidge G.R., =1964ApJ...140.1617B Atlases Galaxy catalogs This electronic version of Arp's 1966 "Atlas of Peculiar Galaxies" contains only its Table 2 published in the Astrophysical Journal Supplement.
Redshifts for galaxies ordered by RA RAh Right Ascension 1970 (hours) h RAm Right Ascension 1970 (minutes) min pPos A closing parenthesis when the original position is parenthesized (APG 238) --- DE- Declination 1970 (sign) --- DEd Declination 1970 (degrees) deg DEm Declination 1970 (minutes) arcmin APG Arp's number --- Name Designation --- Redshifts Values of the redshift with references detailed below --- Francois Ochsenbein CDS 1995 Sep 14 UNKNOWN UNKNOWN * March 1986: Catalogue prepared at CDS * 14-Sep-1995 (version A): documentation added at CDS, a few errors in Arp number corrected. In particular, Table 2 indicates a wrong number for galaxy at 02h37.4 +18 15 which is No.258 (instead of No.254) VII_74A.xml Catalog of Infrared Magnitudes and H I Velocity Widths for Nearby Galaxies 7075 VII/75 Nearby Galaxies - IR Magnitudes and HI widths Catalog of Infrared Magnitudes and H I Velocity Widths for Nearby Galaxies M Aaronson J P Huchra J R Mould R B Tully J R Fisher H van Woerden W M Goss P Chamaraux U Mebold B Siegman G Berriman S E Persson Astrophys. J. Suppl. Ser. 50 241 1982 1982ApJS...50..241A Galaxies, nearby Photometry, infrared H I data The catalog is a compilation of 1.6 micron magnitudes, 21 cm velocity widths, and related data on 308 nearby galaxies. Included are distance relative to the Virgo distance, data sources, group assignments, and notes.
The data name Name NGC designation IC designation UGC (Nilson 1973) designation Coordinate designation preceded by A (Fisher and Tully 1981) Coordinate designation preceded by E (Lauberts et al. 1981, and references cited therein; ESO/Uppsala Survey) --- RAh Right ascension (1950) hours A majority of the positions given were newly determined by Aaronson et al. (1982). Objects without positions measured by the authors of the these authors will have a note indicating the source of the coordinates given. h RAm Right ascension (1950) minutes A majority of the positions given were newly determined by Aaronson et al. (1982). Objects without positions measured by the authors of the these authors will have a note indicating the source of the coordinates given. min RAs Right ascension (1950) seconds A majority of the positions given were newly determined by Aaronson et al. (1982). Objects without positions measured by the authors of the these authors will have a note indicating the source of the coordinates given. s DE- Declination (1950) sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec type Morphological type In the revised Hubble system (de Vaucouleurs et al. 1976; RC2), using the notation of the RC2. --- incli Inclination Generally this was determined from axial ratios. See Aaronson et al. (1982) for details of the method used and for further references. deg mag 1.6 micron magnitude No correction has been applied for internal galactic absorption, but the photometry has been corrected for both galactic extinction and for redshift effect on the isophotal diameter . . . . See Aaronson et al. (1982) for a discussion of the correction applied, of the errors expected, and of the references used in determining this value. mag log_d Log. of isophot. diam. The isophotal diameters . . . are obtained from the RC2, unless noted otherwise . . . . The D1 system is essentially the same as the D0 system of the RC2, differing only in the galactic extinction correction and in the use of a cutoff term applied to objects at high inclination . . . . See Aaronson et al. (1982) for a discussion of the transformations used on data from different sources and of likely sources of error. 0.1arcsec redsh Redshift Measured for neutral hydrogen and stated as a heliocentric velocity in km/sec. km/s width Velocity width HI velocity width, in km/sec, corrected for inclination and (1 + z) expansion effect. See Aaronson et al. (1982) for details of the corrections applied and for a discussion of agreement between observers and of possible sources of error. km/s HI H I flux integral Observed HI flux density integral, in Jy km/sec, corrected for the effects of partial resolution by the telescope beam. See Aaronson et al. (1982) for details of how the data were selected to ensure consistency. Jy/km/ dist Relative distance Ratio of the distance of the galaxy to the distance of Virgo. The distances relative to Virgo are calculated from redshifts and from the infall model discussed in @Aaronson et al. 1982, Astrophys. J., in press; . . . . Because of restrictions imposed by the model used, those galaxies with galactocentric redshifts below 300 km/sec and/or lying within a conical shell between 6 deg. and 25 deg. from Virgo were excluded from these calculations. For these galaxies, this field is blank. --- source Source(s) The source(s) of the HI data listed are cited here by a character code up to three letters long. The corresponding references are listed by code as follows: ADM Aaronson et al. 1981. AHM Aaronson, Huchra, and Mould 1979. CRW Cram, Roberts, and Whitehurst 1980. DR Dickel and Rood 1978. HGR Haynes, Giovanelli, and Roberts 1979 KS Krumm and Salpeter 1979. P Peterson 1979. P1 Aaronson, Mould, and Huchra 1980. P2 Mould, Aaronson, and Huchra 1980. P3 Aaronson et al. 1980. S Shostak 1978. SA Shostak and Allen 1980. TF Fisher and Tully 1981. VW van Woerder et al. 1982. WG Whiteoak and Gardner 1977. --- group Group A group assignment is listed here only if at least two members of the group are present. See Aaronson et al. (1982) for a discussion of how group assignments were determined. --- note Notes Notes are cited by code number. Many galaxies have no notes at all, while some have as many as four. The codes are as follows: 1. Position from de Vaucouleurs and Leach 1981. 2. Position from Gallouet, Heidmann, and Dampierre 1975 (and references cited therein). 3. Morphological type adopted from the UGC. 4. Diameter and axial ratio obtained from the UGC. 5. Morphological type adopted from Nilson 1974. 6. Diameter and axial ratio obtained from Nilson 1974. 7. Morphological type adopted from Lauberts et al. 1981. 8. Diameter and axial ratio obtained from Lauberts et al. 1981. 9. Position from Lauberts et al. 1981. 10.Morphological type assigned by Aaronson et al. (1982). 11.Diameter and axial ratio obtained from mean of Lauberts et al. 1981 and Nilson 1974 data. 12.H-0.5 estimated from average of data and mean growth curve extrapolation. 13.Position from Dressel and Condon 1976. 14.The S0 type in RC2 is a misclassification; spiral arms are clearly visible in the ESO blue plate. --- Nancy G. Roman SSDOO/ADC 1995 Aug 28 UNKNOWN UNKNOWN The catalog was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnee Astronomiques, Strasbourg (CDS), in February 1986. The original tape contained a single text file in a format identical to that of the published paper. An editor was used to expand abbreviations, to reformat the note field, and to compress the data file from 124 to 111-byte records by removing blank columns. The record for object NGC 4124, omitted from the original tape file received by the ADC, was located in the published catalog and re-inserted into this distribution version of the catalog. A FORTRAN program was run that checked the validity of each field according to its data type and value. This work and the preparation of the original document was performed by Anne C. Raugh. The undersigned translated the document from a Script form available in hard copy only to the current ASCII document. VII_75.xml Catalogue of Isolated Pairs of Galaxies in the Northern Hemisphere 7077 VII/77 Isolated Pairs of Galaxies in the Northern Hem Catalogue of Isolated Pairs of Galaxies in the Northern Hemisphere I D Karachentsev Publ. of the Special Astrophy. Observatory of USSR AS, No. 7 ??? ??? 1972 1972SoSAO...7....1K Galaxies The catalog is a compilation of observational data for 603 isolated pairs of galaxies with component magnitudes brighter than 15.7 and north of declination -3 degrees. The catalog includes pair numbers and component letters, coordinates, apparent magnitudes, radial velocities, major axes and eccentricities, Hubble classifications, spectral types, and distances between components.
Catalog Data ID Current number of the pair Running number of the pairs in this catalog. --- Comp A or B for the components Indicates to which component of the pair the data refer. This is always either A or B. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin mag Apparent magnitude mag RV Radial velocity Radial velocity corrected for the Sun's motion km/s e_RV Mean square error on RV km/s r_RV Source of RV Sources of radial velocities are: =1= Karachentsev I.D., 1980, ApJS 44, 137 ; Karachentsev I.D., 1981, Sov. Astron. Letters 7, 76; Karachentsev I.D., 1983, Sov. Astron. Letters 9, 67 =2= White S.D., Huchra J., Latham D., Davis M., 1983, MNRAS 203, 701 =3= Tifft W.G., 1982, ApJS 50, 319 =4= Karachentsev I.D., Sargent W.L.W., Zimmermann B., 1979, Astrofiz. 15, 25 Karachentsev I.D., Pronik V.I., Chuvaev K.K., 1975, A&A 41, 375 Karachentsev I.D., Pronik V.I., Chuvaev K.K., 1976, A&A 51, 185 =5= Rood H.J., 1983, "A catalogue of Galaxy Redshifts"; de Vaucouleurs G., de Vaucouleur A, RC2 catalogue =6= Huchra J., Davis M., Latham D., Tonry J., 1983, ApJS 52, 89 Gregory S.A., 1975, ApJ 199, 1 Khachikjan E., 1973, Astrofiz. 9, 157 --- D Major axis arcmin Eccen Minor-to-major axis ratio --- MType Morphological type in Hubble's classification Hubble types have been chosen as follows: 'E ' : all ellipticals 'S0' : just Hubble S0 type 'Sx' , x=a,b,c: includes SBx 'Sm' : includes Irr --- Sp Spectral type The codes as described in Karachentsev et al. (1985) are 'ABS' : absorption-line system 'WEK' : weak emission 'MID' : medium strength emission 'STG' : strong emission --- Sep Distance between components (min. of arc) arcmin Francois Ochsenbein CDS C.-H. Joseph Lyu Hughes STX/NASA 1997 Jan 27 The original ADC documentation by Anne C. Raugh (1986) was used to generate this ReadMe file. UNKNOWN UNKNOWN The Catalogue of Isolated Pairs of Galaxies in the Northern Hemisphere was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnes Astronomiques, Strasbourg (CDS), in February 1986. The original tape contained only the single text file. (Although Karachentsev et al. (1985) refers to a second file of documentation, this was apparently not included in the data received from the CDS.) An editor was used to compress the data file from 70 to 59-byte records by removing blank columns. The data required no further editing. A FORTRAN program was run that checked the validity of each field according to its data type and value. Addendum (04/27/87): In a private communication dated 18 December 1986 and received by the Astronomical Data Center 23 April 1987, V. Lebedev notes that the Catalogue of Isolated Pairs of Galaxies in the Northern Hemisphere lists several galaxy-star pairs. While these objects have the same coordinates and radial velocities, there is no information for them regarding the type of the galaxy or the type of its linear spectrum. VII_77.xml The HEAO A-1 X-Ray Source Catalog 7080 VII/80 The HEAO A-1 X-Ray Source Catalog The HEAO A-1 X-Ray Source Catalog K S Wood J F Meekins D J Yentis H W Smathers D P McNutt R D Bleach E T Byram T A Chubb H Friedman M Meidav Astroph. Jour. Suppl. 56 507-649 1984 1984ApJS...56..507W X-ray sources The HEAO A-1 X-Ray Source Catalog is a compilation of data for 842 sources detected with the U. S. Naval Research Laboratory Large Area Sky Survey Experiment flown aboard the HEAO 1 satellite. The data include source identifications, positions, error boxes, mean X-ray intensities, and cross identifications to other source designations.
The primary objective of the Naval Research Laboratory (NRL) Large Area Sky Survey Experiment (LASS) flown aboard the HEAO 1 satellite was to conduct an all-sky survey for the brightest X-ray sources in the energy range 0.25 to 25 keV. The instrumentation consisted of an array of large proportional counter modules with collimators of varying fields of view and with sufficient sensitivity to detect sources as faint as 0.25 mu.Jy at 5 keV, assuming a Crab-like spectrum (1.1 muJy at 5 keV = 1 UFU for a Crab-like spectrum). Full sky coverage was achieved in the first 6 months of the mission by continuously scanning great circles perpendicular to the Earth-Sun line. The HEAO A-1 catalog results from the 6-month survey and, thus, covers the whole sky. For additional information concerning the NRL LASS instrument, the data analysis procedures, characteristics and limitations of the source data, and a discussion of X-ray source classes, the source publication should be consulted.
The data name Source designation (1H) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- RA Right ascension (RA) in degrees deg RAh RA (B1950.0) hours h RAm RA (B1950.0) minutes min RAs RA (B1950.0) seconds s DE Declination (Dec) in degrees deg DE- Declination sign --- DEd Dec (1950.0) degrees deg DEm Dec (1950.0) minutes arcmin DEs Dec (1950.0) seconds arcsec glon Galactic longitude deg glat Galactic latitude deg long Ecliptic longitude deg lat Ecliptic latitude deg RA1 Right ascension_1 The source coordinates (center of error box) are given in degrees and in sexagesimal form. The subscripted right ascensions and declinations (right ascension_1-4, declination_1-4) give the positions of the 95 percent confidence error box surrounding each source. All positions are for equinox B1950.0. deg DE1 Declination_1. deg RA2 Right ascension_2 deg DE2 Declination_2 deg RA3 Right ascension_3 deg DE3 Declination_3 deg RA4 Right ascension_4 deg DE4 Declination_4 deg area Area of error box deg2 flux Flux The apparent intensity of the source in counts/sq.cm/s for 0.5 - 25 keV. The determination of the errors is described in Section III of the source reference (Wood et al. 1984). As explained in that paper, an intensity of 10**-3. counts/sq.cm/s, which is the limiting flux in the catalog, corresponds to 3.3*10**-12 ergs/sq.cm/s in 2-10 keV, both for a Crab-like spectrum, meaning that 10**-3 counts/sq.cm/s in HEAO A-1 is equivalent to 0.20 UFU or to 0.22 muJy at 5.2 keV, again for a Crab-like spectrum. cm2/s e_flux Flux error cm2/s name2 Alternate designation (X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name3 Alternate designation (X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name4 Alternate designation (X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name5 Alternate designation (X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name6 Alternate designation (X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name7 Alternate designation (X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name8 Alternate designation (X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name9 Alternate designation (non-X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name10 Alternate designation (non-X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name11 Alternate designation (non-X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- name12 Alternate designation (non-X-ray) The first seven fields (bytes 150-239) contain alternate designations of each source in other X-ray catalogs, while the last four fields are for non-X-ray cross identifications. Catalog identifications and references are given in Table 5 of the source paper. Cross identifications were selected according to certain criteria. For X-ray catalogs (4U, 2A, 1M, etc.), where error boxes of up to several degrees are sometimes reported, the cross reference is given whenever the other error box intersects the HEAO A-1 error box. Identifiers are also given in certain cases where boxes do not strictly intersect but are sufficiently close to suggest a possible relationship. The criterion used is that the separation between box centers must be less than the sum of the two largest dimensions. The designation XRS (not included in Table 5, but described in text) is from Amnuel, Guseinov, and Rakhamimov (1979), 4hich summarizes much of the older X-ray literature. Non-X-ray cross identifications were made on several bases. Whenever an identification has been firmly established, for example, by a precise position from a modulation collimator or from the Einstein Observatory, it is always shown, but so are many additional tentative identifications. Some of these have been suggested by earlier work (in which case the earlier literature appears either in Table 5 or Table 6 of the source reference) and the remainder have been found by searching the non-X-ray catalogs listed by the authors in their Table 5. Additional information on selection criteria will be found on page 647 of the source reference. Whenever an (R) appears in the last field, additional references and comments will be found in Table 6 of the source reference. Those entries are intended primarily to provide a sketch of the basic background and current state of knowledge concerning the sources, to direct users to further literature, and to clarify ambiguities. They are not intended to be a comprehensive bibliography and many references are omitted. A special effort has been made to provide cross references to other HEAO 1 literature wherever possible, since other HEAO 1 observations are simultaneous with and complementary to those in the catalog. --- Nancy G. Roman ADC/SSDOO 1995 May 08 Appreciation is expressed to Kent Wood for communicating about the catalog in 1986 and for supplying multiple copies of the source paper. Dr. Warren also thanks Dr. Wood for reviewing and commenting on a draft version of this document. The help of Jonathan McDowell of the Harvard-Smithsonian Center for Astrophysics is also gratefully acknowledged. Dr. McDowell requested a machine-readable copy of the catalog and made suggestions about the proposed format, including the elimination of the redundant error box positions in sexagesimal form. The catalog was edited and the documentation prepared by Dr. Wayne Warren. It was translated from Script to ASCII and put in the current standard form by the undersigned. UNKNOWN UNKNOWN The HEAO A-1 X-Ray Source Catalog was received on magnetic tape by the National Space Science Data Center on 20 July 1984 from Dr. Kent S. Wood of the Naval Research Laboratory. The tape was in VAX VMS BACKUP format with variable length logical and physical records, plus special control words (logical record length of each record in the first four bytes.) A program was written to convert the records to fixed length and the tape file was processed to disk storage on the IBM 3081 computer of the NASA Space and Earth Sciences Computing Center at GSFC. The format of the file was identical to Table 4 of the published catalog, meaning that there were 10 sources per group (page in the published catalog), separated by column headings and blank records, etc. All blank, text, and separator records were removed with an editor, leaving just four records per source. A format was designed that rearranged the data in logical order for a single record per source structure, and a program was written and executed to reformat the data. The advantages of the single record per source structure are that all records are entirely uniform and the catalog can be sorted and searched easily. The original catalog contained the error box positions in both decimal and sexagesimal form. The latter data were omitted during the conversion in order to decrease the final record length, since the sexagesimal data can be reconstructed easily from the decimal positions given. VII_80.xml Catalogue of Isolated Galaxies 7082A VII/82A Isolated Galaxies Catalogue of Isolated Galaxies V E Karachentseva V S Lebedev A L Shcherbanovskij CDS Bull. No. 30, p. 125 ??? ??? 1986 1986BICDS..30..125K Galaxy catalogs The catalog is a compilation of information on 1051 isolated galaxies with apparent magnitudes brighter than 15.7 and north of declination -3 degrees. New data about the morphological types, the isolation class, and the radial velocities have been added to this version. The catalog includes running numbers for the galaxies, equatorial coordinates, isolation classes, apparent magnitudes, morphological types, major axes, axial ratios, and radial velocities.
Catalog data for 1051 isolated galaxies Num Running number of the galaxy in this catalog --- RAh Right ascension (Equatorial coord. 1950.0) h RAm RA in minutes min DE- Sign of Declination --- DEd Declination (1950) in degrees deg DEm DEC in arcminutes arcmin IsoClass Isolation class Single-digit number in the range 0-2: 0 = Isolated 1 = Marginally isolated 2 = Member of a group or cluster --- Vmag Apparent magnitude mag Mtype Morphological type Morphological type. Two-character code: E = Elliptical S0 = Lenticular SA = Includes SBa SB = Includes SBb SC = Includes SBc SM = Includes Irr --- Maxis Major axis arcmin AxiRatio Axial ratio Ratio of the minor axis to the major axis. --- RadVel Radial velocity km/s e_RadVel Mean square error in the radial velocity km/s r_RadVel Rad. vel. source Two-digit code indicating the source of the radial velocity. The full forms of the references and their corresponding codes are listed in Appendix A. --- C.-H. Joseph Lyu Hughes STX 1995 Paul Kuin [ADC] 13-May-1997 Dec 12 The original ADC documentation by Anne C. Raugh (1987) was used to create this ReadMe file. UNKNOWN UNKNOWN The (CIG) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in December 1986. The original tape consisted of two text files, one containing the catalog data and another containing a short explanation of the catalog fields and the list of radial velocity source references. The only change made to the catalog file was to delete blank columns to reduce the record size from 65 to 52 bytes. Appendix A. - Radial Velocity References 1. Karachentseva, V. E., and Karachentsev, I. D. 1981, Pis'ma Astron. Zh., 7, 195. Karachentseva, V. E., and Karachentsev, I. D. 1979, Astrofizika, 15, 589. Karachentseva, V. E., and Karachentsev, I. D. 1985, Astrofizika, 22, in press. 2. Rood, N. J. 1980, Catalog of Galaxy Redshifts. 3. Huchra, J., Davis, M., Latham, D., and Tanory, J. 1983, Astrophys. J. Suppl., 52, 89. Bothum, G. D., Geller, M. J., Beers, T. C., and Huchra, J. P., CfA Preprint, N 1714. 4. Sandage, A. R. 1978, Astron. J., 83, 904. 5. Haynes, M. P., and Giovanelli, R., 1984, Astron. J., 89, 195. 6. Arakelian, M. A., Dibay, E. A., and Yessipov, V. F. 1972, Astrofizika, 8, 177, 329. 7. Arakelian, M. A., Dibay, E. A., and Yessipov, V. F. 1975, Astrofizika, 11, 377. 8. Arakelian, M. A., Dibay, E. A., and Yessipov, V. F. 1976, Astrofizika, 12, 195. 9. Gueriguene, M. F. 1975, in La Dynamique de Galaxies Spirals. 10. de Vaucouleurs, G., de Vaucouleurs, A., and Corwin, H. 1976, Second Reference Catalogue of Bright Galaxies (Austin: University of Texas). 11. Sargent, W. L. W. 1970, Astrophys. J., 160, 405. 12. Thonnard, N., Rubin, V. C., Ford, W. K., and Roberts, M. 1978, Astron. J., 83, 1564. 13. Barton, R. 1969, Mem. Soc. Astr. Ital., 40, 211. VII_82A.xml Isolated triple galaxies. The complete sample for radial velocities and reduced data. 7083 VII/83 Isolated Triplets of galaxies Isolated triple galaxies. The complete sample for radial velocities and reduced data. V E Karachentseva I D Karachentsev V S Lebedev Astrofiz. Issled. 26 42 1988 1988AISAO..26...42K Galaxy catalogs The complete data for radial velocities of components of triple galaxies are presented. The main part of observations was accomplished with the 6-meter telescope.
Data for the triplets of galaxies Seq Running number --- m_Seq Component in triplet --- Isol Isolation criteria of Karachentsev --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Mag apparent magnitude mag n_Mag (unexplained flag) --- MajAxis Major axis reduced to 25mag/arcsec2 isophote arcmin Min/Maj Ratio MinAxis/MajAxis --- MType Morphological classification --- Sep Separation between the components number=1 separations refer to components: m_Seq = 'A' : A-B m_Seq = 'B' : B-C m_Seq = 'C' : C-A arcmin Geom Geometrical configuration number=2 Geometry is indicated as: T = Triangle D = Double+isolated L = line --- Nopt Number of optical components --- RadVel Radial velocity km/s e_RadVel Mean error on RadVel km/s r_RadVel Reference code number=3 References: 1 = Karachentseva V.E., Karachentsev I.D., Shcherbanovsky A.L, 1979 Astrofiz. Issled. 11, 3 2 = Zwicky F., Herzog E., KArpowicz C.T., Kowal C.T., "Catalogue of Galaxies and Clusters of Galaxies", vols I-VI, California Inst. of Technology 1961-68 3 = Karachentsev I.D., Karachentseva V.E., 1981, Astrofyz. 17, 5 4 = Karachentseva V.E., Karachentsev I.D., 1983, Astrofiz. 19, 613 5 = Karachentsev I.D., Karachentseva V.E., Shcherbanovsky A.L, 1978, Pis'ma Astron. Zh. 4, 483 6 = Karachentsev I.D.,, Karachentseva V.E., Shcherbanovsky A.L, 1985, Astrofiz. Issled. 19, 3 7 = Geller M.J., Huchra J.P., 1983, ApJS 52, 61 8 = Tifft W., 1982, ApJS 50, 319 9 = Baiesi-Pillastrini G.C., Palumbo G.G.C., Vettolani G., 1984, A&AS 56, 363 10 = Rood H.J, 1980, "A catalogue of galaxy redshifts", preprint 11 = Huchtmeier W.K., Richter O.G., et al., 1983, ESO Preprint 250 12 = Karachentseva V.E., 1973, Astrofyz. 8, 3 --- Francois Ochsenbein CDS 1995 Jul 23 UNKNOWN UNKNOWN The catalogue on magnetic tape was received at CDS from Moscow Data Center before the actual publication; the ReadMe file was added in July 1995. VII_83.xml Groups of Galaxies. III. The CfA Survey 7084A VII/84A Groups of Galaxies. III. The CfA Survey Groups of Galaxies. III. The CfA Survey M J Geller J P Huchra Astrophys. Journ. Suppl. 52 61 1983 1983ApJS...52...61G Surveys Galaxy catalogs The catalog contains statistically homogeneous groups of galaxies based on the Harvard-Smithsonian Center for Astrophysics (CFA) redshift survey. Groups in the catalog are all density enhancements in redshift space of a factor greater than 20. All groups contain at least three members. There are 176 groups in the catalog and 102 groups have been identified in one or more previous studies. The catalog includes group numbers, numbers of members, equatorial coordinates, mean flow-corrected galactocentric velocities, line-of-sight-velocity dispersion, integrated group magnitudes, crossing times for the groups, and mean harmonic radii of the groups.
CfA redshift survey data for 176 galaxy groups GrpNum Group running number --- NumGal Number of Galaxies composing this group --- RAh Right Ascension (1950) hours h RAm RA in minutes min DE- Sign of Declination --- DEd Declination (1950) in degrees deg DEm DEC in arcminutes arcmin GCvel GC velocity Mean flow-corrected galactocentric velocity in km/sec. km/s Vdisp LOS vel. disp. Line-of-sight velocity dispersion, uncorrected for measurement error, in km/sec. km/s GrpMag Integrated group magnitude mag CrsTime Crossing time Crossing time of the group in units of 1/H. This field was mislabeled in Geller and Huchra (1983) (see History). H/s Mradius Mean harmonic radius Mean harmonic radius of the group as defined by equation (13) of Huchra and Geller (1982), in Mpc. This field was mislabeled in Geller and Huchra (1983) (see Remarks and Modifications). Mpc Comparing this catalog against 3 earlier ones GrpNum Catalog number of the group --- TGnum TG number(s) Corresponding TG group, if any. This may be a range; for example, 50-57 for GOGIII group 94. --- NBnum Corresponding NB group number --- DVnum Corresponding DV group number --- Alias Other names of groups in this cluster --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Dec 12 The original ADC documentation by Anne C. Raugh (1987) was used to create this ReadMe file. UNKNOWN UNKNOWN The (GOGIII) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in December 1986. The original tape consisted of two text files of data from Tables 1 and 3 in the published catalog Huchra and Geller (1982). Blank columns were removed from Table 1 using an editor to reduce the record size from 54 to 45 bytes. The character "-", used in Table 3 to indicate no data, was changed to a blank, so that most of the fields could be read with a FORTRAN integer format. No other changes were made in either file. A FORTRAN program was run to check the validity of each field according to its data type and value. In the original published catalog (Geller and Huchra 1983) the crossing time and mean harmonic radius fields were mislabeled (erratum, Geller and Huchra 1984). We wish to thank J. P. Huchra for bringing this to our attention. The second file, table3.dat, contains a table comparing the present catalog against three earlier catalogs: DV = de Vaucouleurs (1975); NB = Huchra and Geller (1982); TG = Turner and Gott (1976) VII_84A.xml Systematic Properties of Compact Groups of Galaxies 7085A VII/85A Systematic Properties of Compact Groups of Galaxies Systematic Properties of Compact Groups of Galaxies P Hickson ApJ 255 382 1982 1982ApJ Clusters, galaxy Galaxy catalogs The catalog is a list of 100 compact groups of galaxies identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec and satisfies an isolation criterion. The catalog includes running numbers, equatorial coordinates, group types according to the two brightest members, number of galaxies in the group, angular diameters of the smallest circles containing the geometric centers of all group members, total magnitudes (red) of those galaxies counted as group members, estimated red magnitudes of the brightest galaxies in the groups, corrected redshifts of the brightest galaxies, and other designations of the groups.
Data Num Running number of the group in this catalog --- RAh Equatorial coordinates 1950 Right Ascension h RAm Right Ascension minutes min RAs Right Ascension seconds s DE- Declination sign --- DEd Declination degrees (1950) deg DEm Declination arcminutes arcmin DEs Declination arcseconds arcsec Type Type Two-character code (a letter followed by a number) classifying the group according to its two brightest members: S The brightest galaxy is a spiral galaxy. E The brightest galaxy is not a spiral galaxy. 1 m(b) - m(a) >= 1.0 2 0.5 <= m(b) - m(a) < 1.0 3 m(b) - m(a) < 0.5 where m(a) and m(b) are the estimated red magnitudes of the brightest and second brightest members, respectively, of the cluster. --- MCount Member count Number of galaxies in the group. Only those galaxies within three magnitudes of the brightest galaxy are counted as members. --- AngSize Angular size Angular diameter, in arcminutes, of the smallest circle containing the geometric centers of all group members. arcmin TotMag Total magnitude Total estimated red magnitude of those galaxies counted as group members (see member count, above.) mag Bmag Brightest member magnitude Estimated red magnitude of the brightest galaxy in the group, in units of magnitude. mag Rshift Redshift Corrected redshift of the brightest galaxy. In all but ten cases this field is blank. --- Aname1 Alternate name 1 Other designations of the group, if any (at most, four). --- Aname2 Alternate name 2 --- Aname3 Alternate name 3 --- Aname4 Alternate name 4 --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Oct 16 UNKNOWN UNKNOWN The (SPCGG) was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from the Centre de Donnees Astronomiques, Strasbourg (CDS), in December 1986. The original tape consisted of a single text file containing the catalog data from Table 1 of Systematic Properties of Compact Groups of Galaxies , in a slightly more compact format. ADC personnel deleted eight blank columns from the end of each record in the file to reduce the record size from 80 to 72 bytes and ran a FORTRAN program to check the validity of each field according to its data type and value. Two minor typographic errors discovered in the computer-readable version were then corrected by referring to the published catalog. A possible error was also detected, but not changed, in record number 97, where the DEC seconds field contains a value of 60 (this value appears in the printed version). P. Hickson kindly supplied a list of errata including some corrections in addition to the published erratum. This list is reproduced below; the indicated changes have already been made to the catalog data. ERRATUM No AngSize TotMag Bmag 14 6.7 12.1 13.0 22 5.0 10.5 11.1 60 2.3 13.4 14.4 69 1.9 12.2 13.1 82 3.1 12.2 13.1 No RAh/RAm/RAs DEd/DEm/DEs 03 00 31 39 -07 52 07 31 04 59 08 -04 19 42 74 15 17 14 +21 04 27 89 21 17 34 -04 07 17 AngSize angular size of the group TotMag total magnitude of the group Bmag magnitude of the brightest member VII_85A.xml Groups of Galaxies. I. Nearby Groups 7086A VII/86A Groups of Galaxies. I. Nearby Groups Groups of Galaxies. I. Nearby Groups J P Huchra M J Geller Astrophys. J. 257 423 1982 1982ApJ...257..423H VII/84 : Groups of Galaxies. III. (Geller & Huchra, 1983) VII/164 : The CfA Redshift Catalogue, Version Nov. 1993 (Huchra+, 1993) Huchra, J.P., Davis, M., Latham, D., and Tonry, J. 1982, ApJS, 52, 89 de Vaucouleurs, G. 1975, in Galaxies and the Universe, eds. A. Sandage, M. Sandage, and J. Kristian (Chicago: University of Chicago Press) Clusters, galaxy Galaxy catalogs cosmology: observations galaxies: clusters: general galaxies: distances and redshifts The catalog contains nearby groups of galaxies with outer number density enhancement greater than 20. The groups were searched using a whole sky catalog of 1312 galaxies brighter than mag 13.2 (B) with complete redshift information (Huchra et al. =1983ApJS...52...89H). Only groups containing more than two members are included. The catalogue includes equatorial coordinates, average radial velocities, and velocity dispersions for 92 nearby groups in the first file. A second file contains the results of a comparison between this catalog and de Vaucouleurs' (1975) catalog of nearby groups The Hubble constant was assumed 100km/s/Mpc.
Group Parameters (from Table 5) HGnum Group running number --- Ngal Number of Galaxies composing this group --- RAh Right Ascension (1950) hours h RAm RA in minutes min DE- Sign of Declination --- DEd Declination (1950) in degrees deg DEm DEC in arcminutes arcmin GCvel Mean flow-corrected galactocentric velocity km/s Vdisp Line-of-sight velocity dispersion km/s GrpMag Integrated group magnitude mag H*xTime Crossing time in units of 1/H (Eq. 16) --- Mradius Mean harmonic radius (Eq. 13) Mpc Msep Mean pairwise separation (Eq. 14) Mpc Mgrp Mass of the group (Eq. 15) solMass M/L Mass/Luminosity ratio (Eq. 15) Sun Comparison with de Vaucouleurs (from Table 4) DVnum de Vaucouleurs (1975) group number(s) --- HGnum Group(s) from this paper --- Names Other names of the group --- Joseph Florsch, Francois Ochsenbein CDS 1996 Sep 18 UNKNOWN UNKNOWN The catalogue was prepared at CDS; the first version contained only columns 1-7 of the Table 5 (file groups.dat). The missing columns were added in September 1996 at CDS. The description is from Nancy G. Roman at ADC. VII_86A.xml Data on 1889 Abell's rich clusters of galaxies 7087A VII/87A Data on 1889 Abell's clusters of galaxies Data on 1889 Abell's rich clusters of galaxies A A Leir S van den Bergh Astrophys. J. Suppl. Ser. 34 381 1977 1977ApJS...34..381L VII/110A : (1989 version of Abell's Catalogue) Clusters, galaxy Galaxy catalogs A sample of 1889 clusters from Abell's catalogue of Rich Clusters of Galaxies (1958, ApJS 3, 211) have been classified in the Bautz-Morgan system
Table 1 of the paper, cols 1,6,7,9-11 Abell Abell cluster number --- BMclass Bautz-Morgan class number=1 The classification is written with arabic number, with 1.5 = I-II and 2.5 = II-III. The classification is defined in Bautz L.P., Morgan W.W., 1970, ApJ 162, L149: Class I = clusters containing a centrally located cD galaxy II = clusters where brightest galaxy or galaxies are intermediate in appearance between class cD and the Virgo-type giant ellipticals III = clusters containing no dominant galaxies. --- u_BMclass Uncertainty symbol (:) on BMclass --- AppRadius Apparent cluster radius on the red plate of the Palomar Sky Survey number=2 1 mm = 67.14" mm MajAxis Apparent major axis of the brightest cluster member number=2 1 mm = 67.14" mm MinAxis Apparent minor axis of the brightest cluster member number=2 1 mm = 67.14" mm rmag Photo-red magnitude of the brightest cluster member corrected for absorption. mag Francois Ochsenbein CDS 1995 Jul 21 UNKNOWN UNKNOWN * March 1990: the BMclasses I-II and III were all coded as '3' (note from H. Andernach). The corrections have been made at NSSDC/ADC (version VII/87A) * 21-Jul-1995: Standard description added at CDS VII_87A.xml CEDAG Catalogue of Clusters of Galaxies 7088 VII/88 CEDAG Catalogue of Clusters of Galaxies CEDAG Catalogue of Clusters of Galaxies A Fernandez G Mathez L Nottale Comptes Rendus sur les Journees de Strasbourg, 6eme Reunion, 33, Strasbourg: Observatoire de Strasbourg ??? ??? 1984 VII/4 : Abell and Zwicky Clusters of Galaxies (Abell+ 1974) VII/49 : Galaxies in CGCG (Zwicky, 1968) Abell G. O., 1958. Astrophysics. J. Supp. 3, 211 (see catalog <VII/110>) Fernandez, A., Nottale, L., 1984, Bull. Inform. CDS, 26, 93 Karachentsev, J. D., 1970, Prob. kosm. Fiz. 5, 201 Zwicky, F., Karpowicz, M., Kowal, C. T., Herzog, E., Wild, P., Catalog of galaxies and of clusters of galaxies (CGCG) Calif. Inst. of Techn. 1961-1968 (see catalogs <VII/49> and <VII/4>) Clusters, galaxy Galaxy catalogs This catalog contains for 10411 objects, the Abell, Zwicky, and Kalinkov numbers of groups of galaxies. In addition, it contains: Abell or Zwicky coordinates, the Abell or Zwicky numbers of the supercluster which contains each group, the diameter (Zwicky), the magnitude (Abell), the compactness (Zwicky), the distance of the group (both Abell and Zwicky), the richness (Abell) and the population (Zwicky).
The data for each group RAh Right ascension hours (1950) The positions in bytes 1 to 9 are from Abell if those are available; otherwise they are from Zwicky. In both cases they are rounded to the minute of time or arc. The more specific positions are in bytes 16 to 49. h RAm Right ascension minutes (1950) min DE- Sign of the declination (1950) --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin Abell Abell number --- RAhA Right ascension hours (Abell) h RAmA Right ascension minutes (Abell) min RAsA Right ascension seconds (Abell) s DE-A Sign of Abell declination --- DEdA Declination degrees (Abell) deg DEmA Declination minutes (Abell) arcmin DEsA Declination seconds (Abell) arcsec Zwicky Zwicky number --- RAhZ Right ascension hours (Zwicky) h RAmZ Right ascension minutes (Zwicky) min RAsZ Right ascension seconds (Zwicky) s DE-Z Sign of Zwicky declination --- DEdZ Declination degrees (Zwicky) deg DEmZ Declination minutes (Zwicky) arcmin DEsZ Declination seconds (Zwicky) arcsec Kalinkov Kalinkov number --- sup_ID Abell or Zwicky number of supercluster For galaxies in superclusters, these columns give the number of the corresponding supercluster and of the cluster within that supercluster to which the galaxy belongs. --- clus_ID Abell or Zwicky number of cluster --- diam_d Zwicky diameter (degrees) deg diam_m Zwicky diameter (arcminutes) arcmin mag Magnitude (Abell) mag comp Compactness (Zwicky) --- distA Distance group (Abell) --- distZ Distance group (Zwicky) --- rich Richness (Abell) --- pop Population (Zwicky) --- *Notes on individual groups cat Source: A=Abell; K=Kalinkov If bytes 1-5 are blank, the note is a continuation of the previous line. --- ID The number in that source --- Text Text of the note --- Nancy Grace Roman ADC/SSDOO 1996 Mar 05 UNKNOWN UNKNOWN The following list of catalogs of clusters of galaxies is included in Fernandez et. al. (1984). For each reference, the parentheses contain the type of sources and the data included. These are followed by a number indicating the number of entries. Zwicky F., Karpowicz M, Kowal C. T., Herzog E , Wlld P., Catalog of galaxies and of clusters of galaxies (CGCG) Calif. Inst. of Techn. 1961-1968. (Clusters; Coordinates, distance class, compactness, population, maps) 9700 Abell G.0., 1958. Astrophys. J. Supp. 3. 211 (Clusters - magnitude of tenth brightest galaxy, distance class, richness class) 2712 Klemola A.R., 1969, Astron. J. 74, 804 (Clusters and groups, [south] - coordinates, angular dimensions, population, magnitude, type) 44 Snow T. P. Jr. 1970, Astron. J. 75, 237 (Clusters and groups [south] - Coordinates, angular dimensions, population, magnitude, type) 34 Sersic J.L. 1974. Astrophys. Space Scl. 28, 365 (Clusters and groups [south] - Coordinates, dimension, description) 68 Rose J. A. 1976, Astron Astrophys. Suppl. 23, 109 (Clusters [south] - Coordinates, population, dimensions, type) 124 Duus A., Newell B., 1977 Astrophys. J. Suppl. 75, 209 (Clusters [south] - Coordinates, concentration class, distance class, population) 957 Braid M.K., Mac Gilliwray H. T., 1978, M.N.R.A.S 182, 241 (Clusters [south] - Coordinates, distance class, richness class) 474 Vidal V. N. 1980. Catalogue of very faint clusters of galaxies in the region of the South Galactic Pole (unpublished) (Clusters [south]) Murray S.S., Forman W., Jones C., Giacconi R., 1978, Ap. J. Lett. 219, L89 (Superclusters) 21 Rood H. J. 1976, Ap. J. 207, 16 (Superclusters) 44 Thuan T.X., 1980, "Les Houches" Session XXXII, Cosmologie Physique, p. 277 (Superclusters) 17 Fullerton W., Hoover P., 1972, Ap. J. 172, 9 (Superclusters) 4 Abell G.0., 1961, A.J. 66, 607 (Superclusters) 17 Gusak A.I., 1970, Soviet Physics Astronomy 13, 964 (Superclusters) 9 Rose J.A., 1977, Ap. J. 211, 311 (Compact groups - Coordinates, magnitude, dimensions) 38 Karachentsev J. D., 1970, Prob. kosm. Fiz. 5, 201 (Groups) 63 Hickson P., 1982, Ap. J. 255, 382 (Compact groups - coordinates, number, magnitude, velocity) 100 Huchra J.P., Geller M.J., 1982, Ap. J. 257, 423; Geller M. J., Huchra J.P., 1983, Ap. J. Suppl. 52, 61 (Groups - Coordinates, number of galaxies, radial velocity, velocity dispersion, magnitude, radius, separation, list of individual galaxies) 92, 176 Materne J., 1978, Astron. Astrophys. 63, 401 (Groups) 5 Materne J., 1979, Astron. Astrophys. 74, 235 (Groups) 5 Tully B., 1982, Ap. J. 257, 389 (Groups, clouds) 11 Shakhbazian R. K., 1973, Astrophysics 9, 296 - List I; Shakhbazian R.K., Petrosian M.B., 1974, Astrophysics 10, 6 - List II; Baier F.W., Petrosian M.B., Tiersch H., Shakhbazian R.K., 1974, Astrophysics 10, 202 - List III; Petrosian M.B., 1974, Astrophysics 10, 291 - List IV; Baier F.W., Tiersch H., 1975, Astrophysics 11, 146 - List V; Baier F.W., Tiersch H. 1976, Astrophysics 12, 1 - List VI; Baier F.W., Tiersch H., 1976, Astrophysics 12, 263 - List VII; Baier F.W., Tiersch H., 1978, Astr physics 14, 157 - List VIII; Petrosian M.B., 1978, Astrophysics 14, 356 - List IX; Baier F.W., Tiersch H., 1979, Astr physics 15, 24 - List X; (Compact groups of compact galaxies - Coordinates, [cross-identification], number of galaxies [more than four] [magnitude of the brightest), angular dimension, coefficient of relative compactness.) 377 Einasto J., Joeveer M., Kaasik A., Kalamees P., Vennik J. 1977, Tartu Astron. Obs., Teat Einasto J., Joeveer M., Kaasik A., Kalamees P., Vennik J. 1977, Tartu Astron. Obs., Teated N򠴹 (Hypergalaxies) 60 Vorontsov-Velyaminov B.A., 1959, "Atlas and Catalog of Interacting Galaxies", vol. 1, Sternberg Institute, Moscow State University; 1977, Astron. Astrophys. Suppl. 28, 1, vol. II (Interacting galaxies) de Vaucouleurs G., 1975, in Stars and Stellar Systems vol. IX p. 557, ed. Sandage (Groups - radial velocity, distance modulus, coordinates [galactic, supergalactic], diameters) 54 Turner E.L., Gott J.R.Ill, 1976, Ap. J. Suppl. 32, 409 (Groups - Coordinates, population, angular diameter, total magnitude, radial velocity, velocity dispersion, faint members, contamination [amount]) 103 Shane C.D., Wirtanen C.A., 1967 Pub. Lick Obs. 22, part I (Galaxy counts [Lick]) Seldner N., Siebers B., Groth E.J. Peebles P.J.E., 1977, Astron. J. 82, 249 (Galaxy counts; new reduction of Lick counts (magnitude range) Projects in process: Abell - continuation of Zwicky (Southern clusters) VII_88.xml Catalogue of Open Cluster Data (5th Ed.) 7092A VII/92A Open Cluster Data 5th Edition Catalogue of Open Cluster Data (5th Ed.) G Lynga Lund Observatory ??? ??? 1987 1987 Clusters, open Bibliography Combined data The fifth edition of the Lund Catalogue of Open Cluster Data gives key information for all known open star clusters in this galaxy. As far as possible only published data have been quoted; for some of the parameters, these values have been selected from other references, which are listed. The catalog includes cluster identification, position, reference, Trumpler classification, membership, angular diameter, mean distance, reddening, turn-off color, age, Fe/H, radial velocity, star types, magnitudes, color, number of observed stars, richness class, earliest spectral class, magnitude brightest member, galactocentric distance, linear diameter, and comments. Further errors have been corrected at CDS: see below the "Historical Notes" section. A few questions still remain (see section "Problems" below)
The Catalogue Data File ClSeq Cluster Sequence code number=1 The Cluster Sequence Code has the following values: 1 NGC 2 IC 3 Berkeley 4 Czernik 5 Dolidze 6 Collinder 7 Upgren 8 Tombaugh 9 Ruprecht 10 King 11 Stock 13 Trumpler 14 Markarian 16 Haffner 17 Hogg 18 Sher 19 Feinstein 20 Harvard 21 Lynga 22 Westerlund 23 Basel 24 Blanco 25 Baractova 26 Biurakan 27 Melotte 28 Pismis 30 Trapezium 32 Pleiades 33 Graff 34 Iskudarian 35 Stephenson 36 Roslund 37 Hyades 41 van den Bergh-Hagen 42 Bochum 43 Dolidze-Dzimselejsvili 45 Antalova 46 Moffat 47 Havlen-Moffat 48 Frolov 50 van den Bergh 51 Mayer 52 Latysev 53 Sigma Ori 54 Graham 55 Aveni-Hunter 56 Loden 57 Grasdalen 58 Waterloo 59 Auner 61 Schuster 62 Danks 63 Muzzio 64 =ref.378 --- ClNum Number inside Cluster Sequence number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- RAh2000 Right Ascension 2000 (hours) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. h RAm2000 Right Ascension 2000 (minutes) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. min DE-2000 Declination 2000 (sign) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- DEd2000 Declination 2000 (degrees) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. deg DEm2000 Declination 2000 (minutes) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. arcmin RAh Right Ascension 1950 (hours) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. h RAm Right Ascension 1950 (minutes) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. min DE- Declination 1950 (sign) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- DEd Declination 1950 (degrees) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. deg DEm Declination 1950 (minutes) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. arcmin precRA Precession in RA (for 10 years) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. 0.1min/yr precDE Precession in DE (for 10 years) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. 0.1arcmin/yr GLON Galactic longitude number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. deg GLAT Galactic latitude number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. deg LundRec Record number on Lund disc number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- OCL OCL number (ref.19) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Diam Selected Angular diameter number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. arcmin r_Diam Reference for angular diameter number=7 the unexplained reference (-1) exists for the clusters C0728-168, C0728-169, C1726-324 --- Dist Distance number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. pc r_Dist reference for Distance number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- log.Age log(age), years number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. yr r_log.Age reference for log(age) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- [Fe/H] Metallicity, logarithmic scale number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. Sun r_[Fe/H] reference for metallicity number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- E(B-V) Reddening number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mag r_E(B-V) reference for Reddening number=5 this field is apparently in error, it contains frequently "-1" or "**" --- ClTyp "DO" indicates at doubtful cluster number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- r_ClTyp reference for ClTyp number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(Ap) Number of Ap stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(Am) Number of Am stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(mAp) Number of marginal Ap stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(mAm) Number of marginal Am stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(WR) Number of WR stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(Of) Number of Of stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(Be) Number of Be stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(sh) Number of Shell stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(Be+sh) Number of Be+Shell stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(He-weak) Number of He weak stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(He-rich) Number of He rich stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(Cep) Number of Cepheids number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(PN) Number of Planetary nebulae number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(C*) Number of Carbon stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(LPV) Number of Long period variable stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(dSct) Number of Delta Scuti stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(bCep) Number of Beta Cephei stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(RCrB) Number of R Cor Bor stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(BaII) Number of Ba II stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- N(UGem) Number of ? U Geminorum stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- refN References for numbers of peculiar stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- POSS-type POSS chart type (So/O/E=1/2/3) number=2 this field is always blank. --- POSS POSS chart number number=2 this field is always blank. --- RAhPOSS Right Ascension POSS (hours) number=2 this field is always blank. h RAmPOSS Right Ascension POSS (minutes) number=2 this field is always blank. min DEdPOSS Declination POSS (degrees) number=2 this field is always blank. deg xPOSS Position position on POSS chart, mm number=2 this field is always blank. mm yPOSS Position position on POSS chart, mm number=2 this field is always blank. mm maxDiam Max angular diam, min of arc number=2 this field is always blank. arcmin maxBr Brightest star number=2 this field is always blank. mag TrConc Trumpler concentration class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- TrRange Trumpler Range class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- TrRich Trumpler Richness class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- TrNeb Trumpler nebulosity (n/u/e=1/2/3) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- inRef.128 '1' if cluster is in (ref.128) number=2 this field is always blank. --- POSS.128 '1' if cluster has POSS data in (ref.128) number=2 this field is always blank. --- Diam.50 Selected angular diameter number=2 this field is always blank. arcmin Dist.50 Distance number=2 this field is always blank. pc maxBr.50 Brightest star number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mag Sp.50 Spectral class code number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- totMag.50 Total magnitude number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mag E(B-V).50 Colour excess number=2 this field is always blank. mag inRef.50 '1' if cluster is in (ref.50) number=2 this field is always blank. --- totMag.422 Total magnitude number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mag i(B-V).422 Integrated color (B-V) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mag N.422 Number of stars considered number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Num.265 Janes-Adler star number number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Class.265 Janes-Adler class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Ref.265 Janes-Adler references number=2 this field is always blank. --- maxClass.265 Janes-Adler maximum class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Rich.265 Janes-Adler richness class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- E(B-V).265 Janes-Adler Color Excess E(B-V) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- r_E(B-V).265 Janes-Adler ref. for E(B-V) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- turn.265 Janes-Adler (B-V) turn-off point number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mag r_turn.265 Janes-Adler ref for (B-V) turn-off point number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- TrConc.320 Trumpler concentration class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- TrRange.320 Trumpler range class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- TrRich.320 Trumpler richness class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- TrNeb.320 Trumpler nebulosity class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Members.320 Number of member stars number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Diam.320 Angular diameter number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- POSS-type.320 Survey chart type number=3 the survey may be SO, O, E, J, R, I or SR --- POSS.320 chart number number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- RAhPOSS.320 Right Ascension POSS (hours) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. h RAmPOSS.320 Right Ascension POSS (minutes) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. min DEdPOSS.320 Declination POSS (degrees) number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. deg xPOSS.320 distance from left edge of chart number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mm yPOSS.320 distance from bottom edge of chart number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mm hasClass.320 '1' if cluster classified in ref.320 number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- ESO/SERC '1' if cluster is on ESO/SERC Survey number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- w_RVel Weights for radial velocity number=6 w_RVel has only the values 0.0 or 1.0 --- RVel Radial Velocity number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. km/s RVelClass Weight class for radial velocity number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- r_RVel references for radial velocities number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- RVel.64 Radial Velocity number=2 this field is always blank. km/s Dist.64 Distance number=2 this field is always blank. pc E(B-V).64 E(B-V) number=2 this field is always blank. mag iMag.64 Integrated apparent pg. magnitude number=2 this field is always blank. mag iAbsMag.64 Integrated absolute Bmag number=2 this field is always blank. mag Diam.64 Absolute Diameter number=2 this field is always blank. pc log(age).64 log(age), years number=2 this field is always blank. yr slog.Mass.64 log (Mass), solar masses number=2 this field is always blank. solMas inRef.64 '1' if cluster is in (ref.64) number=2 this field is always blank. --- phSystem.37 Photometric system for following data number=2 this field is always blank. --- E(B-V).37 Colour excess number=2 this field is always blank. mag Av.37 Interstellar extinction number=2 this field is always blank. mag Dist.37 Distance number=2 this field is always blank. pc Sp.37 Spectral type of hottest star number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- ColBlue.37 Colour type of bluest star number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Diam.37 Cluster diameter number=2 this field is always blank. pc ObsType.37 Type of observation number=2 this field is always blank. --- inRef.37 '1' if cluster is in (ref.37) number=2 this field is always blank. --- Diam.487 Apparent Diameter number=2 this field is always blank. arcmin Rich.487 Richness: vp, p, m, r, vr number=2 this field is always blank. --- inRef.487 '1' if cluster is in (ref.487) number=2 this field is always blank. --- Cname [C0-9+-] Cluster "C" designation --- tr-RA tracer for RA, 1950.0 number=8 tracers are indexes of the previous or next entry according to the parameter; it has been omitted for C2357+606 --- tr-GLON tracer for Galactic longitude number=8 tracers are indexes of the previous or next entry according to the parameter; it has been omitted for C2357+606 --- tr-ClNum tracer for number in sequence number=8 tracers are indexes of the previous or next entry according to the parameter; it has been omitted for C2357+606 --- tr+RA tracer for RA, 1950.0 number=8 tracers are indexes of the previous or next entry according to the parameter; it has been omitted for C2357+606 --- tr+GLON tracer for Galactic longitude number=8 tracers are indexes of the previous or next entry according to the parameter; it has been omitted for C2357+606 --- tr+ClNum tracer for number in sequence number=8 tracers are indexes of the previous or next entry according to the parameter; it has been omitted for C2357+606 --- Dist.jdl jdl distance modulus number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. pc w_Dist.jdl weight class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- turn.jdl jdl turn-off point colour number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mag Age.jdl jdl derived age number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. Myr w_Age.jdl weight class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- E(B-V).jdl jdl reddening number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. mag n_E(B-V).jdl 'v' if reddening varies number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- w_E(B-V).jdl weight class number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- [Fe/H].jdl jdl abundance value number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. Sun refs.jdl references for jdl input number= the "C" cluster designation has the general "format" CHHMM+DDd, i.e. starts with the letter 'C', followed by the right ascension (1950) in hours and minutes. followed by the declination sign, degree and tenth of degree. --- Galactic Coordinate File GLON Galactic longitude deg GLAT Galactic latitude deg OCL OCL number (ref.19) --- Cname Cluster name --- Name Cluster Sequence name and number --- LundRec Record number of Lund disc --- intro.doc Original introduction file edited.txt Catalogue Print file (pages of 60 lines) alias.txt Alias file refs.txt Reference File Francois Ochsenbein CDS 1995 Feb 20 UNKNOWN UNKNOWN * Oct-1991: ADC CD-ROM "Selected Astronomical Catalogs" Vol. 1 (directory /nonstell/clusters/open) : see file "intro.doc" * 14-Feb-1995: CDS (Francois Ochsenbein) => file "edited": - removed the duplicated last two clusters C2351+614 and C2353+642 - corrected the (erroneously positive) declinations of C0635-008 C1859-005 C0657-001 C0719-008 => file "catalog": - transformed into a file with 514-byte records; - replaced blank values of 'N(UGem)' with zero; - put sign of declinations in constant column - removed first record with initial tracers - corrected misalignments for C0548+217 - corrected declinations for C0717-010, C0635-008 C1859-005 C0657-001 C0719-008 - corrected positions of C0819-360, C0820-360, C0915-495 and C1654-457 (see below) - added C2357+606 (Berkeley 58, 1st record) which was missing (existed in "edited", but not in "catalog") UNKNOWN UNKNOWN Problems: * Cluster "C2306+606" indicates an unknown '64' ClSeq with '1' number in file "catalog" and blank name in file "edited". It is the only one from ref. 378 (Pfleiderer et al., 1977) * The positions disagreed with galactic position and have been corrected for the following clusters : ------------------------------------------------ Cname Original Position from galactic pos. 1950 (1950) (2000) ------------------------------------------------ C0819-360 820.3-3614 0819.2-3601 0821.1-3611 C0820-360 821.5-3610 0820.2-3559 0822.1-3609 C0915-495 914.1-4947 0915.0-4930 0916.7-4943 C1654-457 1654.3-4551 1654.2-4543 1657.9-4548 ------------------------------------------------ References: Janes K.A., Tilley C., Lynga G., 1988, Astron. J. 95, 771 VII_92A.xml A Palomar Observatory Sky Survey Atlas of Selected Molecular Clouds 7094 VII/94 POSS Atlas of Selected Molecular Clouds A Palomar Observatory Sky Survey Atlas of Selected Molecular Clouds D A Klinglesmith J M Hollis Astrophys. J. Suppl. Ser. 64 127 1987 1987ApJS...64..127K Atlases Nebulae Surveys The atlas contains data digitized from the Palomar Observatory Sky Survey glass plates for 43 cold, dense molecular clouds. Regardless of the clouds' extent, the digitized area is limited to a 22x22 arcmin on the sky with pixel size of 1.3 arcsec. Central coordinates (B1950.0) for each cloud are given. The data and requisite header information for each digitized molecular cloud are formatted in accordance with the Flexible Image Transport System (FITS) standard.
List of regions observed FileName Name of file containing the image (the .fit extension omitted) --- OBJECT Name of central objet --- ObsDate Observation date "DD/MM/YY" RAdeg Center of image (right ascension), B1950 deg DEdeg Center of image (declination), B1950 deg f01.fit W3M f02.fit NGC1333 f03.fit B5-NH3 f04.fit S206 f05.fit S209 f06.fit L1551 f07.fit TMC1 f08.fit ORION-KL f09.fit OMC2 f10.fit NGC1999 f11.fit NGC2023 f12.fit NGC2024 f13.fit L1662 f14.fit S247 f15.fit NGC2264 f16.fit IRC10216 f17.fit L134N f18.fit ROPH-CO f19.fit ROPH-NH3 f20.fit L63 f21.fit B255 f22.fit B68 f23.fit SGRA-NH3 f24.fit SGR-B2 f25.fit M8 f26.fit M16 f27.fit M17SW f28.fit B133-NH3 f29.fit B134-CO f30.fit W49 f31.fit W51 f32.fit B335-NH3 f33.fit G75.84 f34.fit S106-IRS f35.fit W75N f36.fit DR21 f37.fit B361-NH3 f38.fit IC1396 f39.fit IC5146 f40.fit S140 f41.fit NGC7538 f42.fit CAS-A f43.fit NGC7822 Gail L. Schneider SSDOO/ADC Francois Ochsenbein CDS 1996 Jun 18 UNKNOWN UNKNOWN The file "list" was created from the headers of the FITS files. An error in the declination of the image f28 (B133-NH3) was discovered, and the header was corrected. VII_94.xml A catalog of morphological properties of the 2712 Abell clusters 7096 VII/96 Catalog of morphological properties of Abell clusters A catalog of morphological properties of the 2712 Abell clusters M F Struble H J Rood Astrophys. J. Suppl. Ser. 63 555 1987 1987ApJS...63..555S Clusters, galaxy Morphology galaxies: clusters: general galaxies: distances and redshifts galaxies: structure A catalog is presented which contains Rood-Sastry (1971, hereafter RS) morphological types for all 2712 Abell clusters.
Catalog of morphological properties of Abell clusters Abell Abell cluster identification --- n_Abell An '*' indicates that the cluster is not in Abell's (1980) statistical sample --- Dist Distance class as given by Abell (1980) --- nGal Abell's (1980) number count of galaxies --- Radius Radius of the circular observation window which our data were obtained (1mm=67.14") mm RS1 Basic RS type number=1 Basic RS type: cD, B, L, C, F or I --- RS2 Subsidiary property of RS type number=2 Appendage or subscript which indicates a subsidiary property : p=peculiar cD galaxy n=multiple nucleus cD galaxy s=satellite of a cD galaxy b=connected supergiant binary galaxy within a B-type cluster p=peculiarity associated with a supergiant binary galaxy or the B cluster itself a=arc shape of the line of galaxies defining an L-type cluster c=clumpy s=smooth I-type cluster --- RS3 Number of bright galaxies used to determine RS type for both the C and L types --- T1 First brightest cluster galaxy Hubble type --- Sep1a Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm Sep1b Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm T2 Second brightest cluster galaxy Hubble type --- Sep2a Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm Sep2b Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm T3 Third brightest cluster galaxy Hubble type --- Sep3a Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm Sep3b Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm r12 Separation between the first and second most luminous cluster galaxies (1mm=67.14") mm r13 Separation between the first and third most luminous cluster galaxies (1mm=67.14") mm r23 Separation between the second and third most luminous cluster galaxies (1mm=67.14") mm Nb Number of apparent galaxies that are not among the three most luminous cluster galaxies --- Nt Number of apparent triple galaxies not among the three most luminous cluster galaxies --- n_Nt A 'n' indicates that a galaxy with a multiple nucleus is observed in the cluster --- FRS1a Basic RS type for the first subcluster in an F cluster number=1 Basic RS type: cD, B, L, C, F or I --- FRS1b Subsidiary property of RS type of FRS1 number=2 Appendage or subscript which indicates a subsidiary property : p=peculiar cD galaxy n=multiple nucleus cD galaxy s=satellite of a cD galaxy b=connected supergiant binary galaxy within a B-type cluster p=peculiarity associated with a supergiant binary galaxy or the B cluster itself a=arc shape of the line of galaxies defining an L-type cluster c=clumpy s=smooth I-type cluster --- FRS1c Number of bright galaxies used to determine FRS1 RS type for both the C and L types --- FRS2a Basic RS type for the second subcluster in an F cluster number=1 Basic RS type: cD, B, L, C, F or I --- FRS2b Subsidiary property of RS type of FRS2 number=2 Appendage or subscript which indicates a subsidiary property : p=peculiar cD galaxy n=multiple nucleus cD galaxy s=satellite of a cD galaxy b=connected supergiant binary galaxy within a B-type cluster p=peculiarity associated with a supergiant binary galaxy or the B cluster itself a=arc shape of the line of galaxies defining an L-type cluster c=clumpy s=smooth I-type cluster --- FRS2c Number of bright galaxies used to determine FRS2 RS type for both the C and L types --- FRS3a Basic RS type for the third subcluster in an F cluster number=1 Basic RS type: cD, B, L, C, F or I --- F3RS3b Subsidiary property of RS type of FRS3 number=2 Appendage or subscript which indicates a subsidiary property : p=peculiar cD galaxy n=multiple nucleus cD galaxy s=satellite of a cD galaxy b=connected supergiant binary galaxy within a B-type cluster p=peculiarity associated with a supergiant binary galaxy or the B cluster itself a=arc shape of the line of galaxies defining an L-type cluster c=clumpy s=smooth I-type cluster --- F3RS3c Number of bright galaxies used to determine FRS3 RS type for both the C and L types --- Other Other source data number=4 c: presence of a comment concerning the cluster in "notes" file r: continuum radio emission in a passband centered at a frequency of 1400MHz was detected in the survey by Owen et al. (1982) u: the cluster was observed but not detected at the sensitivity limit of 0.10Jy in the 1400MHz radio survey by Owen et al. (1982) v: the cluster is listed in the catalog of Leir and van den Bergh (1977) x: X-ray emission was detected in the HEAO 1 2-6 keV passband survey of Abell clusters by Johnson et al. (1983) z: the redshift of the cluster is contained in the catalog compiled by Struble and Rood (1986a) --- Additional data for resolved F clusters Abell Abell cluster identification --- u_Abell Uncertainty flag on F type of the cluster (RS1 in table1) --- m_Abell Component of the cluster number=1 M for middle --- RS Basic revised RS type --- T1 First brightest cluster galaxy Hubble type --- SepT1a Separation, see note number=2 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm SepT1b Separation, see note number=2 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm T2 Second brightest cluster galaxy Hubble type --- SepT2a Separation, see note number=2 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm SepT2b Separation, see note number=2 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm T3 Third brightest cluster galaxy Hubble type --- SepT3a Separation, see note number=2 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm SepT3b Separation, see note number=2 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively mm r12 Separation between the first and second most luminous cluster galaxies (1mm=67.14") mm r13 Separation between the first and third most luminous cluster galaxies (1mm=67.14") mm r23 Separation between the second and third most luminous cluster galaxies (1mm=67.14") mm Nb Number of apparent galaxies that are not among the three most luminous cluster galaxies --- Nt Number of apparent triple galaxies not among the three most luminous cluster galaxies --- RS1 Basic RS type for the first subcluster --- RS2 Subsidiary property of RS type number=3 Appendage or subscript which indicates a subsidiary property : p=peculiar cD galaxy n=multiple nucleus cD galaxy s=satellite of a cD galaxy b=connected supergiant binary galaxy within a B-type cluster p=peculiarity associated with a supergiant binary galaxy or the B cluster itself a=arc shape of the line of galaxies defining an L-type cluster c=clumpy s=smooth I-type cluster --- RS3 Number of bright galaxies used to determine FRS1 RS type for both the C and L types --- Sep Separation of the components (1mm=67.14") mm m_Sep Component designation --- PA Position angle of the separation vector of the components deg n_PA Component designation --- Com Comments number=4 c: presence of a comment concerning the cluster in "notes" file --- Additional data for Abell clusters with non-cluster population Abell Abell number --- u_Abell Uncertainty flag on the type of the cluster --- n_Abell C: confused, X: probable cluster in the foreground of an Abell cluster --- RS1 Basic RS type number=1 Basic RS type: cD, B, L, C, F or I) --- RS2 Subsidiary property of RS type number=2 Appendage or subscript which indicates a subsidiary property : p=peculiar cD galaxy n=multiple nucleus cD galaxy s=satellite of a cD galaxy b=connected supergiant binary galaxy within a B-type cluster p=peculiarity associated with a supergiant binary galaxy or the B cluster itself a=arc shape of the line of galaxies defining an L-type cluster c=clumpy s=smooth I-type cluster --- RS3 Number of bright galaxies used to determine RS type for both the C and L types --- T1 First brightest cluster galaxy Hubble type --- SepT1a Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively --- T2 Second brightest cluster galaxy Hubble type --- SepT2a Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively --- T3 Third brightest cluster galaxy Hubble type --- SepT3a Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively --- SepT3b Separation, see note number=3 The number following a 'b' or 's' designation is the measured separation (1mm=67.14") between the components of a binary galaxy or between a cD_s_ galaxy ant its nearby satellite, respectively --- r12 Separation between the first and second most luminous cluster galaxies (1mm=67.14") --- r13 Separation between the first and third most luminous cluster galaxies (1mm=67.14") --- r23 Separation between the second and third most luminous cluster galaxies (1mm=67.14") --- Nb Number of apparent galaxies that are not among the three most luminous cluster galaxies --- FRS1a Revised RS type for the first subcluster --- FRS1c Number of bright galaxies used to determine FRS1 RS type for both the C and L types --- FRS2a Revised RS type for the second subcluster --- FRS2c Number of bright galaxies used to determine FRS2 RS type for both the C and L types --- Com Comments number=4 c: presence of a comment concerning the cluster in "notes" file --- Patricia Bauer CDS 1995 Jan 20 Struble M.F., Rood H.J. First prepared by W.H. Warren (ADC/NASA) VII_96.xml A catalog of 2810 nearby galaxies: the effect of the virgocentric flow model on their observed velocities 7098A VII/98A Catalogue of 2810 nearby galaxies A catalog of 2810 nearby galaxies: the effect of the virgocentric flow model on their observed velocities R C Kraan-Korteweg Astron. Astrophys. Suppl. Ser. 66 255 1986 1986A&AS...66..255K Galaxy catalogs catalogs galaxies: clusters: general galaxies: clusters: individual (Virgo) virgocentric flow model Summary of the paper: A catalog of 2810 nearby galaxies has been prepared. The conditions for an inclusion into the catalog ensure that most galaxies for which the effect of the overdensity of the Virgo cluster on their observed redshifts is not negligible are listed. Three main entities define the catalog: 1) a magnitude-limited catalog with BT <= 13.4mag 2) a volume-limited catalog with V0 <= 500 km/s, and 3) a Virgo catalog for galaxies within a 10deg-cone around M87 limited at BT <= 14.95mag In correspondence to a virgocentric nonlinear flow model (Silk, 1974, 1977), distances are calculated for all galaxies in the catalog with known redshifts. A 95% redshift coverage outside the 10deg-cone around M87 and a 73% coverage within this cone provide the same coverage in computed distances. Two sets of distances are listed resulting from two sets of parameters adopted in the model. They are characterized by a local infall motion towards Virgo of vVC = 220 km/s and vVC = 440 km/s, thus bracketing most published determinations of vVC. Distances are in units of the Virgo cluster distance and independent of any assumption on Ho. In addition to the positions, the recession velocities and the calculated distances, morphological types, diameters, axis ratios, apparent blue magnitudes, and absorption-corrected luminosities based on rVC = 21.7Mpc are listed as well.
The catalog of 2810 nearby galaxies Name1 First name --- Erratum Galaxy should be excluded number=1 (Erratum note) Four galaxies should be excluded from this catalog: NGC 1428, UGC 2689, UGC 5247 and A0524+07. The morphology of NGC 1428 suggests that it is a member of the Fornax cluster. The velocity in Jones and Jones (1980, source 61) supports this assumption. It is therefore regarded as the more probable velocity than the low velocities cited in source 33 and 35. The galaxies UCC 2689 and UGC 5247 are also judged to be more distant than implied by their velocities. As these three galaxies are fainter than the required magnitude limit of this catalog, they should be excluded. The galaxy with the coordinates RA = 05 24.8 and Dec = 07 29 is not visible on the POSS prints. --- Name2 Second name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin MType Coded Morphological type number=2 Morphological Type Coding: The 11 bytes of the MType column are coded as follows (each byte represented by its offset): +00 Special Remark: P pseudo outer ring C cD-galaxy D d (dwarf) for E, S0, S and I R outer ring M merger ? ? +01 Uncertainties concerning byte +00: U preceding description is in (...) ? preceding description is followed by ? +02 Basic type: B BCD, blue compact dwarf D cD galaxy E E F E/S0 K S0/E L S0 S S (S0a - Sm) I I - E-SO, Amorphous + SO/a-Im P Peculiar +03 Bar: A no bar B bar X S/SB or SAB Y S(B) +04 Subtype for S0: 1 1 2 1/2 3 2 4 2/3 5 3 6 1/3 +05 Ellipticity of S0: values 1 to 9, and Z (10) + (+) +06 Inner ring structure: S (s) R (r) T (sr) Q (rs) +07 Further description of main galaxy type (ellipticity for E, lateness of spiral type for S and I): ------------------------------ for E for S for I ------------------------------ 0 E0 S0/a Amorphous 1 E1 Sa Irr II 2 E2 Sab 3 E3 Sb 4 E4 Sbc 4 E5 Sc 6 E6 Scd 7 E7 Sd 8 Sdm 9 Sm Im ------------------------------ +08 Uncertainty of byte +07: : the previous description is followed by : ? the previous description is followed by ? U the previous description is in parentheses (...) +09 Uncertainty of whole morphological type: : whole type description is followed by : ? whole type description is followed by ? U whole type description is in parentheses (...) V whole type description is in brackets [...] +10 Peculiarities: P pec B (pec) F pec: G pec? --- m_MType indicates a second type number=3 For alternative or double descriptions only: R "or" + "and" / "/" --- MType2 Coded second morphological type number=2 Morphological Type Coding: The 11 bytes of the MType column are coded as follows (each byte represented by its offset): +00 Special Remark: P pseudo outer ring C cD-galaxy D d (dwarf) for E, S0, S and I R outer ring M merger ? ? +01 Uncertainties concerning byte +00: U preceding description is in (...) ? preceding description is followed by ? +02 Basic type: B BCD, blue compact dwarf D cD galaxy E E F E/S0 K S0/E L S0 S S (S0a - Sm) I I - E-SO, Amorphous + SO/a-Im P Peculiar +03 Bar: A no bar B bar X S/SB or SAB Y S(B) +04 Subtype for S0: 1 1 2 1/2 3 2 4 2/3 5 3 6 1/3 +05 Ellipticity of S0: values 1 to 9, and Z (10) + (+) +06 Inner ring structure: S (s) R (r) T (sr) Q (rs) +07 Further description of main galaxy type (ellipticity for E, lateness of spiral type for S and I): ------------------------------ for E for S for I ------------------------------ 0 E0 S0/a Amorphous 1 E1 Sa Irr II 2 E2 Sab 3 E3 Sb 4 E4 Sbc 4 E5 Sc 6 E6 Scd 7 E7 Sd 8 Sdm 9 Sm Im ------------------------------ +08 Uncertainty of byte +07: : the previous description is followed by : ? the previous description is followed by ? U the previous description is in parentheses (...) +09 Uncertainty of whole morphological type: : whole type description is followed by : ? whole type description is followed by ? U whole type description is in parentheses (...) V whole type description is in brackets [...] +10 Peculiarities: P pec B (pec) F pec: G pec? --- n_MType Coded Remarks on Morphological Type number=4 Morphological type remarks are: B (double) C (compact) D (dust) J (Jet) L (late) M (merger) N (nearly on edge) O (on edge) P (prolate) R (ring) S (spindle) T (tides) V (very early) 3 (triple) ? follows remark, e.g.(prolate?) --- LClass Luminosity class number=5 the Luminosity class is coded as follows: 1.0 I main class 1.5 I-II 2.0 II 2.5 II-III 3.0 III 3.5 III-IV 4.0 IV 4.5 IV-V 5.0 V 2.2 II.2 intermediate class 3.3 III.3 etc. --- u_LClass Uncertainty of Luminosity class number=6 Uncertainty of luminosity class: : luminosity class is followed by : ? luminosity class is followed by ? U luminosity class is in parentheses (...) V luminosity class is in parentheses (...): W luminosity class is in parentheses (...:) --- logD25 Diameter at 25mag/arcsec2 isophote [0.1arcmin] n_logD25 Note on the computation of logD25 number=7 the following flags are used for logD25 and logR25: 'A' means that logD25 is derived from effective aperture diameter (ref.39) 'B' for estimations from the VCC (ref.BST) --- logR25 Axis ratio log R25 --- n_logR25 Note on the computation of logR25 number=7 the following flags are used for logD25 and logR25: 'A' means that logD25 is derived from effective aperture diameter (ref.39) 'B' for estimations from the VCC (ref.BST) --- HVel Heliocentric velocity number=8 the publication lists the velocity corrected for the solar motion with respect to the local group km/s u_HVel Uncertainty flag on HVel --- e_HVel Error of velocity km/s BT Apparent Blue magnitude BT mag u_BT Uncertainty flag on BT --- n_BT Note if BT not in RC2 system number=9 the flags are 'P' photographic magnitudes 'Z' uncorrected Zwicky magnitudes 'A' unexplained flag in record #245 (MAFFEI II) --- Ai Internal absorption correction A mag n_Ai for low galactic latitude galaxies number=10 the correction for galactic absorption Ao is unreasonably large for galaxies flagged with an '*'. The colon and question marks indicate larger uncertainties. --- r_MType Source of type (see file "refs") --- r_HVel Source of velocity (see file "refs") --- r_BT Source of BT (see file "refs") --- Rem Remarks --- r220(1) First distance in 220 model number=11 Distances are expressed in units of the Virgo Cluster (VC) distance. The models are characterized by a local infall motion toward Virgo of 220km/s and 440km/s respectively. --- n_r220(1) Local group galaxy number=12 galaxies of the Local Group are adopted from Kraan-Korteweg and Tamman (1979), assuming a distance of the Virgo cluster of 21.7Mpc. --- r220(2) Second solution of 220 model number=11 Distances are expressed in units of the Virgo Cluster (VC) distance. The models are characterized by a local infall motion toward Virgo of 220km/s and 440km/s respectively. --- n_r220(2) Local group galaxy number=12 galaxies of the Local Group are adopted from Kraan-Korteweg and Tamman (1979), assuming a distance of the Virgo cluster of 21.7Mpc. --- r220(3) Third solution of 220 model number=11 Distances are expressed in units of the Virgo Cluster (VC) distance. The models are characterized by a local infall motion toward Virgo of 220km/s and 440km/s respectively. --- n_r220(3) Local group galaxy number=12 galaxies of the Local Group are adopted from Kraan-Korteweg and Tamman (1979), assuming a distance of the Virgo cluster of 21.7Mpc. --- r440(1) First distance in 440 model number=11 Distances are expressed in units of the Virgo Cluster (VC) distance. The models are characterized by a local infall motion toward Virgo of 220km/s and 440km/s respectively. --- n_r440(1) Local group galaxy number=12 galaxies of the Local Group are adopted from Kraan-Korteweg and Tamman (1979), assuming a distance of the Virgo cluster of 21.7Mpc. --- r440(2) Second solution of 440 model number=11 Distances are expressed in units of the Virgo Cluster (VC) distance. The models are characterized by a local infall motion toward Virgo of 220km/s and 440km/s respectively. --- n_r440(2) Local group galaxy number=12 galaxies of the Local Group are adopted from Kraan-Korteweg and Tamman (1979), assuming a distance of the Virgo cluster of 21.7Mpc. --- r440(3) Third solution of 440 model number=11 Distances are expressed in units of the Virgo Cluster (VC) distance. The models are characterized by a local infall motion toward Virgo of 220km/s and 440km/s respectively. --- n_r440(3) Local group galaxy number=12 galaxies of the Local Group are adopted from Kraan-Korteweg and Tamman (1979), assuming a distance of the Virgo cluster of 21.7Mpc. --- Keys to source data Ref Reference number --- Text Text of reference --- Francois Ochsenbein CDS 1995 Aug 23 UNKNOWN UNKNOWN * The original tape was received at CDS in 1987 from the author * 23-Aug-1995: (at CDS) The original version with 3 lines per entry was converted into a version with all parameters on a single line, and the standardized description was added. During this process, a few errors were detected and corrected: => misaligned data and/or missing decimal points have been corrected in records 675, 869, 1314, 1513, 1516, 1573, 1745, 2786 ; => an extra digit in u_BT column existed and was removed (replaced by a blank) in the two records: #2517 (NGC 6500), digit '2'; #2518 (NGC 6501), digit '0'; => The four galaxies listed in the Errata have been flagged in byte 11. The references listed in the publication were gathered in the file "refs". VII_98A.xml Catalogue of Radial Velocities of Galaxies 7099 VII/99 Radial Velocities of Galaxies Catalogue of Radial Velocities of Galaxies G G C Palumbo G Tanzellanitti G Vettolani Gordon and Breach Eds. 1983; revised ??? ??? 1986 Galaxy catalogs Radial velocities This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.
Catalogue of radial velocities of galaxies RAh Right Ascension 1950 (hours) number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. h RAm Right Ascension 1950 (minutes) number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. min RAs Right Ascension 1950 (seconds) number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. s DE- Declination 1950 (sign) number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. --- DEd Declination 1950 (degrees) number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. deg DEm Declination 1950 (minutes) number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. arcmin Name Galaxy name the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. --- oType Type of observation: Radio or Optical number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. --- --- Matching left parenthesis number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. --- RV Heliocentric radial Velocity number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. km/s u_RV Wrong or low confidence RV W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity --- e_RV Mean error on RV number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. km/s dRV Galactic correction to RV number= the NGC number is always given first if present ; the Index Catalogue (IC) number follows whenever applicable. Other names listed: ZW : Zwicky lists of compact galaxies (Zwicky and Zwicky, 1971, Zurich; Zwicky et al., 1975AJ.....80..545Z). ZW-S indicates Zwicky's southern survey. MRK : Markarian galaxies, DDO : David Dunlap Observatory galaxies (van den Bergh 1959PDDO....2..145V and 1966AJ.....71..922V) ARP : Arp peculiar galaxies (catalog <VII/74>) VV : Vorontsov-Velyaminov interacting objects (1959, Moscow ; 1977A&AS...28....1V) KDG : Karachentsev double galaxies (cat. <VII/77>) HOL : Holmberg double and multiple galaxies (1937AnLun...6....1H) M : Messier numbers 3CR : Radiogalaxies (see Spinrad, 1985PASP...97..932S) A : in a very few cases, anonymous classification has been used as in the RC1 (Reference catalogue of Bright Galaxies, de Vaucouleurs and de Vaucouleurs, 1964). number= W: Measurement that was successively recognized as wrong by the author(s). These values, although unreliable, have been included in order to prevent the reader from using them. ): (parenthesized value): low confidence in quoted velocity number= references are only available in the printed version of the catalog. number= the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. km/s r_RV Reference number references are only available in the printed version of the catalog. --- Com Comments the following compact comments may occur: *: When an asterisk appears a note is present at the end of the catalogue (available in the printed version only). SEYF: Seyfert galaxy. Sources for this classification are Khachikian and Weedman (1974ApJ...192..581K), Weedman (1977ARA&A..15...69W), Markarian (1977A&A....58..139M) as well as more recent spectral information given in some of the references quoted. DIS: Discrepant velocity. It indicates that the quoted velocity differs by more than 750km/s (i.e., five times a formal optical error of 150km/s) from the first reported velocity, usually a 21-cm high accuracy measurement. If the velocity of the galaxy is greater than 10,000km/s the flag indicates a 3000km/s discrepancy. Some of the discrepancies in RV can be ascribed to serious errors such as inappropriate line identification in the spectra or misidentification of the object. HII REG or KNOT: This is not a morphological comment about the structure of the galaxy. It simply indicates that the reported spectrum was taken on a bright knotty region of the galaxy rather than on its nucleus. These comments may be incomplete due to lack of details in published papers. If this comment appears on the first line it implies that all radial velocities listed under those coordinates refer to the same HII region or Knot. Radial velocities referring to the nucleus of the galaxy containing that HII region or Knot appear under a separate heading. F G: This label identifies galaxies in the optical field of a radiosource that are not associated with the radio source itself, although their coordinates in this catalogue could be the same as those of the radiosource. XYZ: Peculiar names. In order not to overcrowd Column 3, some peculiar names given to galaxies either historically or by their discoverer are given in this column. All Messier's numbers for instance, are given here. All names (shortened in this column) are listed in full in Appendix 9.1 of the printed catalogue. In the case of groups, only the western component is identified; the other components follow. This also holds for groups given in the appendices. --- Francois Ochsenbein CDS 1996 Jul 12 Thanks are due to Dr Giorgio G.C. Palumbo, who kindly supplied the catalog on magnetic tape to CDS in November 1986. UNKNOWN UNKNOWN The printed version was published in 1983 (c) 1983 Gordon and Breach, Science Publishers, Inc. but the electronic version is dated 1986. VII_99.xml Compilation of the Fifth Volume of Morphological Catalogue of Galaxies (-33 to -45deg) 7100 VII/100 MCG Vol.5 Compilation of the Fifth Volume of Morphological Catalogue of Galaxies (-33 to -45deg) B A Vorontsov-Velyaminov V P Arkhipova Trudy Gosud. Astron. Inst. Sternberg 46 ??? ??? 1974 1974TrSht..46....1V VII/62 : MCG parts I to IV (zones +90 to -33deg) Lauberts, A. 1982, The ESO/Uppsala Survey of the ESO(B) Atlas, European Southern Observatory (Cat. <VII/34>) Longo, G., Vaucouleurs, A. de, and Corwin, H.G. 1983, A General Catalogue of Photoelectric Magnitudes and Colours in the U,B,V System, Univ. Texas Kogoshvili, N.G. 1983, CDS Bull. No. 25, p. 63 (Cat. <VII/90>) Vaucouleurs, G. de, Vaucouleurs, A. de, and Corwin, H. 1964, Reference Catalogue of Bright Galaxies, Univ. Texas Vaucouleurs, G. de, Vaucouleurs, A. de, and Corwin, H. 1976, Second Reference Catalogue of Bright Galaxies, Univ. Texas (Cat. <VII/112>) Vorontsov-Velyaminov, B.A., and Arkhipova, V.P. 1974, Morphological Catalogue of Galaxies, V. 5, Moskow Univ. (Cat. <VII/62>) Galaxy catalogs Morphology The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.
The catalogue MCG Morphological Catalog of Galaxies number --- NoteFlag '*' if additional information is given --- Name Galaxy ID: NGC, IC, or A (anonymous) --- RAh Hours RA, epoch 1950.0 h RAm Minutes RA, epoch 1950.0 min RAs Seconds RA, epoch 1950.0 s DE- Sign Dec, epoch 1950.0 --- DEd Degrees Dec, epoch 1950.0 deg DEm Minutes Dec, epoch 1950.0 arcmin mag Integral magnitude (not known for MCG-07-04-003) mag q_mag Accuracy of mag: '1' if magnitude reported to 0.01, '2' id reported to 0.1, '3' if magnitude reported to 1mag --- r_mag Magnitude reference code, see refs.dat --- MajAxisIn Major axis of galaxy bright inner part arcmin MinAxisIn Minor axis of galaxy bright inner part arcmin SurfBrIn Surface brightness of galaxy inner part (Ref 1) --- MajAxis Major axis of galaxy arcmin MinAxis Minor axis of the galaxy arcmin u_MajAxis ':' for uncertain MinAxis or Majaxis --- SurfBrOut Surface brightness of galaxy outer regions (Ref 1) --- Incl Inclination to the line of sight (Ref 1) --- MajAxisMax Maximum major axis (Ref 10 or 256) arcmin MinAxisMax Maximum minor axis (Ref 10 or 256) arcmin DiamCode Code for uncertainty in diameters number=1 Parameter, estimating the uncertainty as follows: '0' for certain values '1' for uncertain values on the blue prints only '2' for uncertain values on the red prints only '3' for uncertain values on the red and blue prints --- PosAng Position angle (Ref 10 or Ref 256) deg q_PosAng Code for uncertainty in PosAng number=2 Parameter, estimating the uncertainty as follows: '0' for certain values '1' for uncertain values '2' for face-on spirals '3' for asymmetric systems --- GalCode Appearance of galaxy number=11 Description of the general appearance of a galaxy according to MCG (ref. 1): Field structure: A B C D E A Description of the general appearance of a galaxy by means of symbols: E,P,L,F B Description of various structure details coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| A. A |I. I |O. 2 |F. F |N. 8 |T. T |B. B | A.D. 5 |E. E |M. M |Z. Z |C. C |A.I. 6 |A 1 | W. W |L. 9 |D. D |B.I. 7 |P. P |? 4 | C the same as B D Type of the faint galaxy seen in contact with the main one, or *, if a star is projected on the image of a galaxy E Structure of the faint galaxy or its inclination to the line of sight. in the case of * in D there are used codes: 1 - for a star, projected on the nuclear region of a galaxy, 2 - on the outer region, 3 - a star is close-by to a galaxy, 4 - a star is possibly projected on the galaxy image --- GalCodeIn Description of gal. inner part, number=12 Description of the galaxy inner bright region according to mcg (ref.1) Field structure: A B C D A Number of galaxy nuclei seen in contact B Description of the galaxy inner region by symbols: N,L,N.. in the case of 'N.' the symbol $ is used on the tape C,D structure of a nuclear region, for () is used the code 3 --- GalCodeOut1 Description of gal. outer part 1 number=13 Description of the galaxy external region according to MCG (ref.1) Description of the external part of a galaxy was carried out from the central regions outwards for five similar areas. For lack of information the corresponding areas were filled with blanks. Field structure for one of the above mentioned similar 5 areas: A B C D E F G A area separating symbols according to MCG, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape| , , |; ; |;; 1 |-> 2 | B number of structure details described in C. In the case of B=9, B must be considered as duplication of symbols in C C Description of galaxy external areas by symbols, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| S S |H H |B B |T T |CAM 6 |R R |L. 9 | C C |SS.S.4 |D D |L L |R. @ |S. 2 | MCG tape|MCG tape|MCG tape| 'REVERSE SS.S.'3 |'REVERSE S.'+S.0 |'REVERSE S' # | 'REVERSE S.' 1 |'REVERSE S'+S 5 |'ARCS' 8 | D,E,F Description of various structure details (the same as B in note (11), as well as the following codes: K - for a galaxy with sharp edges, X - for the traces of structure, Q - for the uncertainty in the number of arms G Uncertainties in structure details coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| ' 1 |(') 4 |->R R |- 2 |->8 8 |() 3 |(-) 6 | --- GalCodeOut2 Description of gal. outer part 2 number=13 Description of the galaxy external region according to MCG (ref.1) Description of the external part of a galaxy was carried out from the central regions outwards for five similar areas. For lack of information the corresponding areas were filled with blanks. Field structure for one of the above mentioned similar 5 areas: A B C D E F G A area separating symbols according to MCG, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape| , , |; ; |;; 1 |-> 2 | B number of structure details described in C. In the case of B=9, B must be considered as duplication of symbols in C C Description of galaxy external areas by symbols, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| S S |H H |B B |T T |CAM 6 |R R |L. 9 | C C |SS.S.4 |D D |L L |R. @ |S. 2 | MCG tape|MCG tape|MCG tape| 'REVERSE SS.S.'3 |'REVERSE S.'+S.0 |'REVERSE S' # | 'REVERSE S.' 1 |'REVERSE S'+S 5 |'ARCS' 8 | D,E,F Description of various structure details (the same as B in note (11), as well as the following codes: K - for a galaxy with sharp edges, X - for the traces of structure, Q - for the uncertainty in the number of arms G Uncertainties in structure details coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| ' 1 |(') 4 |->R R |- 2 |->8 8 |() 3 |(-) 6 | --- GalCodeOut3 Description of gal. outer part 3 number=13 Description of the galaxy external region according to MCG (ref.1) Description of the external part of a galaxy was carried out from the central regions outwards for five similar areas. For lack of information the corresponding areas were filled with blanks. Field structure for one of the above mentioned similar 5 areas: A B C D E F G A area separating symbols according to MCG, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape| , , |; ; |;; 1 |-> 2 | B number of structure details described in C. In the case of B=9, B must be considered as duplication of symbols in C C Description of galaxy external areas by symbols, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| S S |H H |B B |T T |CAM 6 |R R |L. 9 | C C |SS.S.4 |D D |L L |R. @ |S. 2 | MCG tape|MCG tape|MCG tape| 'REVERSE SS.S.'3 |'REVERSE S.'+S.0 |'REVERSE S' # | 'REVERSE S.' 1 |'REVERSE S'+S 5 |'ARCS' 8 | D,E,F Description of various structure details (the same as B in note (11), as well as the following codes: K - for a galaxy with sharp edges, X - for the traces of structure, Q - for the uncertainty in the number of arms G Uncertainties in structure details coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| ' 1 |(') 4 |->R R |- 2 |->8 8 |() 3 |(-) 6 | --- GalCodeOut4 Description of gal. outer part 4 number=13 Description of the galaxy external region according to MCG (ref.1) Description of the external part of a galaxy was carried out from the central regions outwards for five similar areas. For lack of information the corresponding areas were filled with blanks. Field structure for one of the above mentioned similar 5 areas: A B C D E F G A area separating symbols according to MCG, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape| , , |; ; |;; 1 |-> 2 | B number of structure details described in C. In the case of B=9, B must be considered as duplication of symbols in C C Description of galaxy external areas by symbols, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| S S |H H |B B |T T |CAM 6 |R R |L. 9 | C C |SS.S.4 |D D |L L |R. @ |S. 2 | MCG tape|MCG tape|MCG tape| 'REVERSE SS.S.'3 |'REVERSE S.'+S.0 |'REVERSE S' # | 'REVERSE S.' 1 |'REVERSE S'+S 5 |'ARCS' 8 | D,E,F Description of various structure details (the same as B in note (11), as well as the following codes: K - for a galaxy with sharp edges, X - for the traces of structure, Q - for the uncertainty in the number of arms G Uncertainties in structure details coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| ' 1 |(') 4 |->R R |- 2 |->8 8 |() 3 |(-) 6 | --- GalCodeOut5 Description of gal. outer part 5 number=13 Description of the galaxy external region according to MCG (ref.1) Description of the external part of a galaxy was carried out from the central regions outwards for five similar areas. For lack of information the corresponding areas were filled with blanks. Field structure for one of the above mentioned similar 5 areas: A B C D E F G A area separating symbols according to MCG, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape| , , |; ; |;; 1 |-> 2 | B number of structure details described in C. In the case of B=9, B must be considered as duplication of symbols in C C Description of galaxy external areas by symbols, coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| S S |H H |B B |T T |CAM 6 |R R |L. 9 | C C |SS.S.4 |D D |L L |R. @ |S. 2 | MCG tape|MCG tape|MCG tape| 'REVERSE SS.S.'3 |'REVERSE S.'+S.0 |'REVERSE S' # | 'REVERSE S.' 1 |'REVERSE S'+S 5 |'ARCS' 8 | D,E,F Description of various structure details (the same as B in note (11), as well as the following codes: K - for a galaxy with sharp edges, X - for the traces of structure, Q - for the uncertainty in the number of arms G Uncertainties in structure details coded as follows: MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape|MCG tape| ' 1 |(') 4 |->R R |- 2 |->8 8 |() 3 |(-) 6 | --- r_MType1 Ref for MType1: 'U' if from Ref 10; 'R' if from Ref 21, 158 --- MType1 Gal morph. type, de Vaucouleurs class. number=14 Morphological type of a galaxy by de Vaucouleurs classification according to RCBG (Ref.21), or UGC (Ref.10) Field structure: A B C D E F G A Existence of outward ring B,C,D,E Galaxy type F,G peculiarities --- MType2 Gal morph. type, Morgan class. number=15 Type of a galaxy by Morgan's classification according to RCBG (Ref.21) Field structure: A B C D E F A,B,C Galaxy type D,E Spectral class F peculiarities --- MType3 Gal morph. type, from UGC or RCBG number=16 Type of a galaxy by Hubble's classification according to UGC (Ref.10), or van den Bergh's classification according to RCBG (Ref.21) Field structure: A B C D E F G H For the case of Hubble's classification (Ref.10), we have: A,B,E,F Galaxy type coded as follows: UGC tape|UGC tape|UGC tape|UGC tape| E E |E0 E0 |S S |SO SO | SB SB |SBO S1 |P P |IR.R. I | DWARF 1 |DWARF S 2 |DWARF I 3 |DWARF E 4 | DWARF P 5 |S(R) SR |SB(R.) S2 |SBO(R) S3 | S(R)O S4 | C,G Structure details coded as follows: UGC tape|UGC tape|UGC tape|UGC tape|UGC tape| A. A |B. B |A.-B.1 |C. C |B.-C.2 | D. D |C.-D.3 | D Additional symbols coded as follows: UGC tape|UGC tape|UGC tape|UGC tape|UGC tape| : : |? 1 |/ / |(//) 2 |- 3 H Luminosity class: For the case of van den Bergh's classification (rEF.21), we have: A,B Galaxy type C Structure details D Peculiarities, additional symbols E,F,G Characteristics of spiral arms H Luminosity class --- r_MType3 Ref for MType3: 'U' if from Ref 10; 'R' if from Ref 21, 158; 'L' if from Ref 256. --- RV Radial velocity referred to the sun km/s r_RV Radial velocity reference code --- RVcorr Radial velocity corrected for solar motion km/s r_RVcorr Corrected radial velocity reference code --- SN_Date1-1900 Date of 1st supernova explosion a SN_Date2-1900 Date of 2nd supernova explosion a SN_Cnt Number of supernovae observed in galaxy --- U-B Integrated U-B color mag r_U-B U-B reference code --- B-V Integrated B-V color mag r_B-V B-V reference code --- (U-B)0 Integrated "face on" (U-B)(0) color from RCBG mag (B-V)0 Integrated "face on" (B-V)(0) color from RCBG mag Spectrum Integral spectrum --- NucType Type of the nuclear region, Byurakan class. --- n_Spectrum If '1' emission lines in spectrum (Ref 54) --- Member Membership in multiple systems number=17 Appearance of a galaxy in binary or multiple system Field structure: A B C D A The following codes are used: 1 the galaxy has a companion with MCG identification number 2 the galaxy has a companion with no MCG identification number 3 for more than one galaxy in a system described by one MCG identification number B designation of members in binary and multiple systems 1 for the brightest member in a multiple system K for one of the fainter members in a multiple system 2 for one of the members of binary system D for another member of binary system 3 for the brightest member of triple system T for one of the fainter members of triple system C If A=1, then C=XXX (MCG number of the component in the field, positions 8-10), otherwise blank D Degree of isolation of galaxy pairs according to Karachentsev (Ref.57), coded as follows: Ref.57 tape| Ref.57 tape| Ref.57 tape| Ref.57 tape| +,+ 1 | -,- 2 | +,- 3 | -,+ 4 --- Interact Existence of interaction features number=18 Existence of the interaction features Field structure: A B C D E A Number of the members observed in interaction B the following codes are used: if B then interaction is evident if Q then interaction is suspected, otherwise blank C Type of interaction, coded as follows: if 1 then galaxies are connected with a bar if 2 then a galaxy is connected with another one by a spiral arm if 3 then contact of galaxies if 4 then contact of galaxy nuclei if 5 then a nest of galaxies if 6 then a chain of galaxies if 7 then galaxies are embedded in common nebulous envelope D Description of apparent galaxy form distortion by means of codes: if 1 then existence of a tail if 2 then existence of unusual branched features (jet, streamer, plume, etc.) if 3 then a halo if 4 then clear evidence of structure distortion if 7 then galaxies are embedded in common nebulous envelope E Angular separation of members in system in minutes of arc (E=X.X) --- Comp Existence of faint components number=19 Existence of faint components Field structure: A B C D A Number of faint components B the following codes are used: 1 a galaxy has a faint component with MCG identification number 2 a galaxy has a faint component with no MCG identification number 3 a galaxy has a faint galaxy close-by 4 a galaxy has a questionable object (star or defect), close-by C either MCG number of a component in the field (if B=1), or a magnitude of a nearest component (if B=2,3,4). C=XX D angular distance to the nearest companion in minutes of arC. D=X.X --- References RefNo Reference number --- Text Text of reference and remarks (on several lines) --- descr.doc Original Description by N.G.Kogoshvili Francois Ochsenbein CDS 1994 Nov 17 UNKNOWN UNKNOWN * From the CD-ROM "Selected Astronomical Catalogs" Vol. 1 (1992), directory "nonstell/galaxies/mcg5") * 17-Nov-1994 (CDS): The "catalog.dat" file differs from the CD-ROM "mcg5.dat" file: the contents of bytes at the right of #243 were erroneous on the CD-ROM. VII_100.xml Catalogue of Star Clusters and Associations. III. Open Clusters 7101A VII/101A Star Clusters/Associations. III. Open Clusters Catalogue of Star Clusters and Associations. III. Open Clusters J Ruprecht B Balazs R E White Akademiai Kiado, Publ. House Hungarian Acad. Sciences, Budapest ??? ??? 1981 1981 Catalogue of Star Clusters and Associations. III. Open Clusters J Ruprecht B Balazs R E White Soviet Astronomy 27 358 1983 1983SvA....27..358R VII/5 : Excerpt of the Catalogue VII/31 : Part I (Associations) VII/44 : Part II (Globular Clusters) Clusters, open This catalogue includes the Open Clusters of the supplement up to 1973 of the "Catalogue of Star Clusters and Associations" by Alter G., Ruprecht J., Vanysek V., Budapest 1970. The file "main.dat" contains the original data. For each cluster, the first line contains the running number (OCL) followed by various designations. The first five figures represent the galactic longitude (in 0.01degree), 'N' or 'S' for North or South galactic hemisphere, and galactic latitude (in 0.01degree). The second line contains the 1950 coordinates, the 50-yr precession, the galactic direction cosines and the position on the POSS charts. For each cluster a number of bibliographic records follow containing: YEAR: Year of the literature reference NAME: Author PUBLICATION: Reference AD: Angular diameter of the cluster in arc minutes DIST: Distance of the cluster (pc) LD: Linear diameter of the cluster (pc) N: Number of stars studied CI: Color index SP: Spectra P: Positions RV: Radial velocity (km/s) MT: Integrated magnitude NOTE: Notes The file "clusters" has been created from first and second lines; missing equatorial coordinates were derived from the galactic ones.
List of the open clusters OCL Cluster name starting with GCL number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. --- Page Card (or page) number of the second edition number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. --- Name Other name of the association number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. --- GLON Galactic longitude The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. deg GLAT Galactic latitude number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. deg RAh Right Ascension 1950 (hours) number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. h RAm Right Ascension 1950 (minutes) number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. deg DEm Declination 1950 (minutes) number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. arcmin POSS Palomar Sky Survey chart with its RA and Dec number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. --- X Position on the chart from lower left corner number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. mm Y Position on the chart from lower left corner number= The position is missing for the last 5 moving clusters. The equatorial coordinates have been computed from galactic ones for additional clusters, i.e. OCL names with decimal figures. mm Main catalog and bibliography ref The bibliography --- Francois Ochsenbein CDS C.-H. Joseph Lyu, P.Kuin NASA/ADC 1996 Jul 12 UNKNOWN UNKNOWN The file "clusters" was generated at CDS as explained above; the longitude of OCL-105 was corrected, and also the right ascension of OCL-279. At the ADC the Declination of OCL-843.1 and of OCL-852.1 were corrected (Jul 1996). VII_101A.xml Spectrophotometric Atlas of Standard Stellar Spectra 7102 VII/102 Spectrophotometric Atlas of Standard Stellar Spectra Spectrophotometric Atlas of Standard Stellar Spectra A J Pickles ApJS 59 33 1985 1985ApJS...59...33P Spectrophotometry Photometry Continuous spectrophotometry has been obtained for 200 objects at a resolution of 10-17 A over the wavelength region 3600-1000 A. Kron-Cousins BVRI colors are computed for the spectra and compared with published photoelectric photometry. The (V-R)_C color index is used to group the individual observations to form standard spectra types by stellar class. The standard groups include a solar abundance sequence of most spectral types and luminosity classes, metal-rich and metal weak G-K giant-branch sequences, and horizontal-branch giants. The standard spectra are presented in FITS files. The relationship between the file names and the spectral types of the stars is given in the File Summary below.
f01.fit OV, 3A/pix (Spectral type and spectral sampling in Angstroms per pixel) f02.fit B1-3V, 3A/pix f03.fit B4-5V, 3A/pix f04.fit B6-9V, 3A/pix f05.fit A0-3V, 3A/pix f06.fit A4-6V, 3A/pix f07.fit A7-F1V, 3A/pix f08.fit F2-4V, 3A/pix f09.fit F5-6V, 3A/pix f10.fit F7-8V, 3A/pix f11.fit G0-4V, 3A/pix f12.fit G5-8V, 3A/pix f13.fit K0-1V, 3A/pix f14.fit K2-3V, 3A/pix f15.fit K4-7V, 3A/pix f16.fit M0-2V, 3A/pix f17.fit M3V, 3A/pix f18.fit M4V, 3A/pix f19.fit M5-6V, 3A/pix f20.fit Early GIV, 3A/pix f21.fit Mid-GIV, 3A/pix f22.fit Late GIV, 3A/pix f23.fit BIII, 3A/pix f24.fit Early AIII, 3A/pix f25.fit A7-F0III, 3A/pix f26.fit Late FIII, 3A/pix f27.fit G5-9III, 3A/pix f28.fit K0-1III, 3A/pix f29.fit K2III, 3A/pix f30.fit K3III, 3A/pix f31.fit K4III, 3A/pix f32.fit K5III, 3A/pix f33.fit M0-2III, 3A/pix f34.fit M3III, 3A/pix f35.fit M4III, 3A/pix f36.fit M5III, 3A/pix f37.fit M6III, 3A/pix f38.fit mrG5K0III, 3A/pix f39.fit mrK1-2III, 3A/pix f40.fit mrK3III, 3A/pix f41.fit mrK4III, 3A/pix f42.fit mrK5III, 3A/pix f43.fit HBIII, 3A/pix f44.fit wkF0III, 3A/pix f45.fit wkG5III, 3A/pix f46.fit wkG8III, 3A/pix f47.fit wkK0-2III, 3A/pix f48.fit wkK3-4III, 3A/pix f49.fit OV, 12A/pix f50.fit B1-3V, 12A/pix f51.fit B4-5V, 12A/pix f52.fit B6-9V, 12A/pix f53.fit A0-3V, 12A/pix f54.fit A4-6V, 12A/pix f55.fit A7-F1V, 12A/pix f56.fit F2-4V, 12A/pix f57.fit F5-6V, 12A/pix f58.fit F7-8V, 12A/pix f59.fit G0-4V, 12A/pix f60.fit G5-8V, 12A/pix f61.fit K0-1V, 12A/pix f62.fit K2-3V, 12A/pix f63.fit K4-7V, 12A/pix f64.fit M0-2V, 12A/pix f65.fit M3V, 12A/pix f66.fit M4V, 12A/pix f67.fit M5-6V, 12A/pix f68.fit Early GIV, 12A/pix f69.fit Mid-GIV, 12A/pix f70.fit Late GIV, 12A/pix f71.fit BIII, 12A/pix f72.fit Early AIII, 12A/pix f73.fit A7-F0III, 12A/pix f74.fit Late FIII, 12A/pix f75.fit G5-9III, 12A/pix f76.fit K0-1III, 12A/pix f77.fit K2III, 12A/pix f78.fit K3III, 12A/pix f79.fit K4III, 12A/pix f80.fit K5III, 12A/pix f81.fit M0-2III, 12A/pix f82.fit M3III, 12A/pix f83.fit M4III, 12A/pix f84.fit M5III, 12A/pix f85.fit M6III, 12A/pix f86.fit mrG5-K0III, 12A/pix f87.fit mrK1-2III, 12A/pix f88.fit mrK3III, 12A/pix f89.fit mrK4III, 12A/pix f90.fit mrK5III, 12A/pix f91.fit HBIII, 12A/pix f92.fit wkF0III, 12A/pix f93.fit wkG5III, 12A/pix f94.fit wkG8III, 12A/pix f95.fit wkK0-2III, 12A/pix f96.fit wkK3-4III, 12A/pix Gail L. Schneider SSDOO/ADC Seth W. Digel SSDOO 1997 Aug 26 VII_102.xml Catalogue of Galactic Globular Clusters 7103 VII/103 Galactic Globular Clusters Catalogue of Galactic Globular Clusters R Monella Coelum LIII, 287 ??? ??? 1985 Clusters, globular The catalogue collects, for the first time, the most important data concerning all the galactic globular clusters still well known. Here the objects enclosed in famous publications like the ones of Arp (1965), Alter et al. (1970), Alcaino (1973) are reported, with the addition of new clusters noticed recently (TER, ESO, UKS, TJ) and till KOD 1, found by K. Kodaira in July 1983 (IAUC 3846). The most important disposable data in literature have been found about every object. For the clusters found recently, the data may be fragmentary and susceptible of variations. A particular care has been utilized in the research of the most reliable informations and data, that have been homogenized and put in order later on.
Catalog Data ID Running number --- Constel Constellation of belonging --- Name Common name of the globular cluster --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin V Photovisual apparent integrated magnitude mag Mv Photovisual absolute integrated magnitude mag Sp Spectral integrated class --- [Fe/H] Degree of metallicity --- AppDiam Photographic apparent diameter arcmin RealDiam Real diameter pc m(BS) Apparent magnitude of the brightest star mag d-galaxy Distance from the center of our Galaxy kpc d-sun Distance from Sun kpc ConClas Concentration class according to Sawyer-Hogg --- RV Radial velocity km/s N(var) Number of var. stars found in the cluster --- Note (?) --- Francois Ochsenbein CDS ; C.-H. Joseph Lyu Hughes STX/NASA 1996 Sep 26 R. Monella Sharru Astronomical Observatory, Via Giovanni XXIII, 13, 24050 COVO (Bergamo), Italy UNKNOWN UNKNOWN The distance d of cluster#8 was corrected from 16.4 to 116.4kpc to agree with the publication. VII_103.xml Open Cluster Interstellar Matter (OCISM) Database 7106 VII/106 Open Cluster Interstellar Matter Database Open Cluster Interstellar Matter (OCISM) Database D T Leisawitz NASA Ref. Publ. 1202 ??? ??? 1988 1988NASAR1202....1L Clusters, open Interstellar gas Interstellar dust, Interstellar clouds This catalog is a compilation of the characteristics of 128 open clusters and the interstellar medium associated with them. It is distributed as the "OCISM Database" which is the set of data files, processing and analysis software written in FORTRAN, and the supporting documentation. As provided by the author, the data are in a multi-record format which is best accessed with the author's software. The clusters in this database have been relatively well-studied, have declinations greater than minus 20 deg., are between 1 and 5 kpc distant, and are younger than 100 million years old. Characteristics compiled for these clusters include cluster identification, spatial coordinates, radial velocities (of stellar clusters, H II regions, and molecular clouds), proper motions, distance, angular diameter, linear diameter, age, mass (based on stellar and atomic gas, ionized gas, molecular clouds, and dust determinations), visual extinction, and reddening.
ocdbdesc.txt Author's description of OCISM database ocdb.ref Coded list of references James E. Gass SSDOO/ADC 1998 Oct 19 VII_106.xml Asteroids II 7108C VII/108C Asteroids II Machine-Readable Data Base Asteroids II R P Binzel T Gehrels M S Matthews The Univer. Arizona Press, Tucson, p. 997 ??? ??? 1989 1989 Asteroids This data set was assembled by E. F. Tedesco, Jet Propulsion Laboratory, in March 1988 from files provided by the contributors to the above reference. Included are asteroid names and discovery circumstances, proper elements and family identifications, asteroid lightcurve parameters, asteroid pole determinations, taxonomic classes, absolute magnitudes and slope parameters, UBV color indices, and albedos and diameters from the IRAS Asteroid and Comet Survey. The asteroid discovery tables were updated by F. Pilcher in 1994.
The Asteroids 11 data base presented herein is a compilation of asteroid data published, or in press, as of March 1988 with some updates in early 1989 except, as mentioned, the asteroid discovery tables. It is by no means all-inclusive. Excluded are data sets which have remained essentially unchanged since their publication in Asteroids (Gehrels 1979). These include the spectral reflectance and spectral parameter data sets (Chapman and Gaffey 1979), and the polarimetric and groundbased radiometric data sets (Morrison and Zellner 1979). The primary changes from the book are the omission of the asteroid proper elements by Z. Knezevic and A. Milani. A few columns in other tables were omitted of added. The new discovery data set was assembled by E. F. Tedesco, Jet Propulsion Laboratory, in March 1988. The discovery file has been updated twice and the possibility exists that some of the other files were updated prior to publication or will be updated in the future. For this reason, references to data obtained from these files should reference them explicitly. For example a reference to the rotation data base might read "Lagerkvist, C.-I., Harris, A.W., and Zappala, V. (1987). Asteroids II machine-readable data base: acquired from the ADC (catalog 7108C) in December 1997" in the references section. Naturally, a datum on an individual asteroid, at least one you are discussing in detail, should reference the original source. Although an attempt has been made to provide the information required to provide a minimum understanding of the data, the researcher is urged to refer to the more detailed discussions in the published volume.
Names and discovery circumstances num Number of minor planet --- name Name of minor planet --- pre_name Preliminary name --- year Year of discovery yr mon Month of discovery yr/12 day Day of discovery (in month) d dis_name Name of discoverer --- dis_pl Place of discovery --- note Reference to note Notes referencing two or more discoverers with names of combined length too great to fit in the discoverer column, to give a more complete description of programs involving several persons, and to reference cases in which two numbered planets were subsequently discovered to be identical and the number and name of one of these was re-assigned to a newly discovered planet. Notes have also been used to reference conflicting discovery claims and list important independent discoveries which are no longer regarded as official. --- MPC Reference to Minor Planet Cir. References the Minor Planet Circular or Circulars in which information concerning the discovery circumstances and/or name assignment, and occasional error corrections, was first published. The author first listed these references only on 1988 Feb 2 with the publication of MPC 12781. Previously this table had been maintained without references to the original literature. Adding references from earlier publications remains a task for the future (if ever). Would anyone else like to contribute to this important assignment? --- The notes for discover.dat ID Note number If bytes 1-3 are blank, the note is a continuation of the preceding line. --- note Note --- Proper elements and family identities ID Asteroid number --- a Semimajor axis of orbit AU e Eccentricity --- sin_i Sine of inclination --- wbar Proper longit. of perihelion (1950.0) deg anode Proper long., ascending node (1950.0) deg dwbar Rate of longitude of perihelion arcsec/a dnode Rate of longitude of node arcsec/a res Note indicating resonance or sp. case See proper.txt. This is particularly important if this field is not blank. --- dMars Closest colinear distance to Mars AU dJup Closest colinear distance to Jupiter AU u_ID Quality code for Palomar-Leiden astr. Quality code reserved for Palomar-Leiden asteroids. Values 1, 2, 3, 4, X, 0 are in decreasing order of accuracy. see Palomar-Leiden survey for details. A blank, not a zero, is used for numbered asteroids. --- family Family identity if appropriate --- r_ID Reference number --- Lightcurve parameters ID Asteroid number --- name Asteroid name --- n_per Limit sign for period --- per Period The period for 288 Glauke is 1150. and is in the bytes 28-32. h n_mag_1 Limit sign for mag_1 --- mag_1 First mag., amplitude or variation mag lim Separator or limit sign --- mag_2 Second mag., amplitude or variation mag n_mag_2 Uncertainty note on mag_2 --- n_mag Reliability code The Reliability Codes are as follows: 1 = Very tentative result, may be completely wrong. 2 = Reasonably secure result, based on over half coverage of the lightcurve. 3 = Secure result, full lightcurve coverage, no ambiguity of period. 4 = Multiple apparition coverage, pole position reported. --- rem Remarks code The Remarks Codes are as follows: 3 = Number of extrema per rotation cycle (e.g., 1, 3). Unless otherwise noted, two per cycle is assumed. A = Ambiguous period. The "most likely" period is listed, with other possibilities listed in a footnote ordered by asteroid number, below. D = Rotation period "determined" from published data, but not given by author(s) of original data. F = Footnote, below, ordered by asteroid number, containing additional information. N = No lightcurve published. P = Photographic photometry. V = Visual photometry. --- r_ID Reference codes All references to the asteroid are cited by number in the reference file, in chronological order. The last few citations are the most recent, and should be the most useful for evaluating the current state of knowledge of a given asteroid. --- References file for lightcrv.dat ID Reference number If ID is blank, the record is a continuation of the preceding record. --- ref Reference --- Pole determinations ID Asteroid number --- n_ID Source of basic data A = Amplitudes of lightcurves; D = Individual data-points of photometric lightcurves; E = Epochs (e.g., times of lightcurve extreme); F = Fourier coefficients of photometric lightcurves; I = Infrared pre- and post-opposition differences; M = Magnitudes (usually at maximum light); O = 0ccultation observations; P = Infrared polarimetry; R = Radar observations; S = Speckle interferometry; V = Visual position angles; Z = Zero and nonzero amplitude apparitions implying pole-on view in former case. --- par1 Possible parenthesis --- RA_pole Right ascension of pole Pole Coordinates are given in the ecliptical reference frame of equinox 1950. deg u_pole indicates discordant positions --- DE-_pole Declination of pole - sign --- DE_pole Declination of pole deg n_pole Possible parenthesis or discord --- spin_dir Spin direction The sense of rotation is termed indeterminate (1) when the spin direction is known, but the accuracy of the pole coordinates is insufficient to give an unambiguous sense of rotation, or the pole is so close to the ecliptic and/or orbital plane that forced precession will cause the sense of rotation to alternate with time. --- par2 Possible parenthesis --- par3 Possible parenthesis --- RA2_pole Right ascension of pole deg DE2-_pole Declination of pole - sign --- DE2_pole Declination of pole deg spin_dir2 Spin direction --- par4 Possible parenthesis --- n_pole2 Note on pole position A = concentric ring region B = aspect circle C = at least one pole position rejected --- rot Sense of rotation - = Sense of rotation not determined; P = Prograde rotation; R = Retrograde rotation; I = Indeterminate case. M = Moving --- per Period of rotation d n_per Mean of discordant periods = * --- u_per indicates discordant periods --- par7 Possible parenthesis or limit --- a/b Model axial ratio --- par8 Possible parenthesis --- par5 Possible parenthesis --- b/c Model axial ratio --- par6 Possible parenthesis --- n_shape Note on shape * = Mean value of two significantly different solutions (or discordant shape?) ? = One or both shapes questionable E = flat region F = see ref. G = "kettle" H = rnd. cyl. J = complex --- r_ID Reference codes --- References for pole.dat ID Reference identification If ID is blank, the record is a continuation of the preceding record. --- ref Reference --- Taxonomic classifications ID Asteroid number --- name Asteroid name --- Th_cl Tholen class The following notation appears in the classifications: U suffix indicating an unusual spectrum; falls far from cluster center : suffix indicating noisy data :: suffix indicating very noisy data --- indicates data that are too noisy to permit classification (essentially all types would be allowed) --- n_Th_cl Uncertainty note on Th_cl --- Bar_cl Barucci class --- group Asteroid group Due to popular demand, orbital group designations have been included in this table. The 2- or 3-letter abbreviations stand for the following groups: ATE Aten APO Apollo AMO Amor MC Mars crosser HUN Hungaria PHO Phocaea GRI Griqua CYB Cybele HIL Hilda TRO Trojan --- n_ID Note on asteroid 1: 13 Egeria. Tholen (1984) listed classification as CG. C eliminated on the basis of 24-color data. 2: 192 Nausikaa. Tholen (1984) listed classification as RS. R eliminated on the basis of 24-color data. 3: 344 Desiderata. Tholen (1984) listed classification as CSU. SU eliminated on the basis of 24-color data. 4: 515 Athalia. Tholen (1984) listed classification as U. Changed to I as explained in the introduction to the printed article. on the basis of 24-color data. 5: 3200 Phaethon. From Tholen (1985) 6: 3551 1983 RD, 3352 1983 SA, and 1984 BC. Unpublished data of Tholen cited in Hartmann et al. (1987). 7: 3908 1980 PA and 4055 1985 DO2. From Tholen et al. (1988) 8: 1975 U2. Not a proper provisional designation. Data taken from TRIAD UBV table as published by Bowell et al. (1979). In turn, they took the data from unpublished observations by Tedesco. It is not known what this object really is. --- Mag, colors, albedos, and diameters ID Minor planet number Asteroids numbered through 3318 are included. There is one record for each asteroid. --- Mag Mean visual absolute magnitude The visual absolute magnitude from the IRAS ground-based input data set. These differ from the blue absolute magnitudes (HB) given in final data product No. 4. In many cases they also differ from those published in the 1988 Russian ephemeris. mag slope Slope parameter The slope parameter from the IRAS ground-based input data set. In many cases these differ from those published in the 1988 Russian ephemeris. mag q_slope Quality of slope (3 highest) The quality code for the absolute magnitude and slope parameter. 3 is best and 1 worst. --- U-B U-B color The U-B color index from IRAS Asteroid and Comet Survey final data product 13. The quality codes for the UBV colors were obtained as follows: Quality Code For sigma 0 > 0.05 magnitude 1 <= 0.05 but > 0.03 magnitude 2 <= 0.03 but > 0.02 magnitude, and 3 <= 0.02 magnitude 4 <= 0.02 magnitude and good agreement between results from references 1 and 2. mag q_U-B Quality of U-B --- B-V B-V color mag q_B-V Quality of B-V --- r_B-V Source of colors The reference for the UBV color(s): 1 = Bowell et al. (1979) In Asteroids (T. Gehrels, ed.), pp. 1108-1129. ("TRIAD") 2 = Zellner et al. (1985) Icarus 61, 355-416. ("ECAS") 3 = Weighted mean of values from references 1 and 2. --- albedo Visual geometric albedo Visual geometric albedo from IRAS Asteroid and Comet Survey final data product No. 4 --- e_albedo Standard deviation of albedo One sigma formal uncertainty in the visual geometric albedo from IRAS Asteroid and Comet Survey final data product No. 4 --- diam Diameter Diameter (in km) and one sigma uncertainty from IRAS Asteroid and Comet Survey final data product No. 4 km e_diam Standard deviation of diameter km sight Number of sightings Number of IRAS observations used in computing the albedo and diameter (from IRAS Asteroid and Comet Survey final data product No. 4) --- discover.txt *Additional information on discover.dat lightcrv.txt *Additional information on lightcrv.dat pole.txt *Additional information on pole.dat taxonomy.txt *Additional information on taxonomy.dat N.G. Roman ADC/SSDOO 1997 Oct 03 VII_108C.xml A Catalog of IRAS Observations of Large Optical Galaxies 7109 VII/109 IRAS Observations of Large Optical Galaxies A Catalog of IRAS Observations of Large Optical Galaxies W Rice C J Lonsdale B T Soifer G Neugebauer E L Kopan L A Llyod T De Jong H J Habing Astrophys. J. Suppl. Ser. 68 91 1988 1988ApJS...68...91R Galaxies, optical Infrared sources The catalogue reports the observations of 85 galaxies listed in RC2 with apparent blue light isophotal diameters (D25) greater than 8'; there are 83 corresponding maps (NGC 205 and M31 are in one field as are M81 and M82) listed in file "summary". The surface brightness maps have been written to tape in FITS format, as 83 sets of maps, each set consisting of an image and a noise map for each of the four IRAS wavelength bands, leading to 664 FITS images.
Summary of Maps File Number related to file name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec nZa Number of pixels in Z direction at 12um --- nYa Number of pixels in Y direction at 12um --- pixZa Pixel size in Z direction at 12um arcmin pixYa Pixel size in Y direction at 12um arcmin nZb Number of pixels in Z direction at 25um --- nYb Number of pixels in Y direction at 25um --- pixZb Pixel size in Z direction at 25um arcmin pixYb Pixel size in Y direction at 25um arcmin nZc Number of pixels in Z direction at 60um --- nYc Number of pixels in Y direction at 60um --- pixZc Pixel size in Z direction at 60um arcmin pixYc Pixel size in Y direction at 60um arcmin nZd Number of pixels in Z direction at 100um --- nYd Number of pixels in Y direction at 100um --- pixZd Pixel size in Z direction at 100um arcmin pixYd Pixel size in Y direction at 100um arcmin OType Observation type: PO = pointed observation, SS = all-sky Survey Scan --- Name Galaxy name (N=NGC, I=IC) --- f01a.fits Field N 45 at 12um f01an.fits Field N 45 at 12um (noise) f01b.fits Field N 45 at 25um f01bn.fits Field N 45 at 25um (noise) f01c.fits Field N 45 at 60um f01cn.fits Field N 45 at 60um (noise) f01d.fits Field N 45 at 100um f01dn.fits Field N 45 at 100um (noise) f02a.fits Field N 55 at 12um f02an.fits Field N 55 at 12um (noise) f02b.fits Field N 55 at 25um f02bn.fits Field N 55 at 25um (noise) f02c.fits Field N 55 at 60um f02cn.fits Field N 55 at 60um (noise) f02d.fits Field N 55 at 100um f02dn.fits Field N 55 at 100um (noise) f03a.fits Field N 134 at 12um f03an.fits Field N 134 at 12um (noise) f03b.fits Field N 134 at 25um f03bn.fits Field N 134 at 25um (noise) f03c.fits Field N 134 at 60um f03cn.fits Field N 134 at 60um (noise) f03d.fits Field N 134 at 100um f03dn.fits Field N 134 at 100um (noise) f04a.fits Field N 147 at 12um f04an.fits Field N 147 at 12um (noise) f04b.fits Field N 147 at 25um f04bn.fits Field N 147 at 25um (noise) f04c.fits Field N 147 at 60um f04cn.fits Field N 147 at 60um (noise) f04d.fits Field N 147 at 100um f04dn.fits Field N 147 at 100um (noise) f05a.fits Field N 185 at 12um f05an.fits Field N 185 at 12um (noise) f05b.fits Field N 185 at 25um f05bn.fits Field N 185 at 25um (noise) f05c.fits Field N 185 at 60um f05cn.fits Field N 185 at 60um (noise) f05d.fits Field N 185 at 100um f05dn.fits Field N 185 at 100um (noise) f06a.fits Field M 31 at 12um f06an.fits Field M 31 at 12um (noise) f06b.fits Field M 31 at 25um f06bn.fits Field M 31 at 25um (noise) f06c.fits Field M 31 at 60um f06cn.fits Field M 31 at 60um (noise) f06d.fits Field M 31 at 100um f06dn.fits Field M 31 at 100um (noise) f07a.fits Field N 247 at 12um f07an.fits Field N 247 at 12um (noise) f07b.fits Field N 247 at 25um f07bn.fits Field N 247 at 25um (noise) f07c.fits Field N 247 at 60um f07cn.fits Field N 247 at 60um (noise) f07d.fits Field N 247 at 100um f07dn.fits Field N 247 at 100um (noise) f08a.fits Field N 253 at 12um f08an.fits Field N 253 at 12um (noise) f08b.fits Field N 253 at 25um f08bn.fits Field N 253 at 25um (noise) f08c.fits Field N 253 at 60um f08cn.fits Field N 253 at 60um (noise) f08d.fits Field N 253 at 100um f08dn.fits Field N 253 at 100um (noise) f09a.fits Field SMC at 12um f09an.fits Field SMC at 12um (noise) f09b.fits Field SMC at 25um f09bn.fits Field SMC at 25um (noise) f09c.fits Field SMC at 60um f09cn.fits Field SMC at 60um (noise) f09d.fits Field SMC at 100um f09dn.fits Field SMC at 100um (noise) f10a.fits Field N 300 at 12um f10an.fits Field N 300 at 12um (noise) f10b.fits Field N 300 at 25um f10bn.fits Field N 300 at 25um (noise) f10c.fits Field N 300 at 60um f10cn.fits Field N 300 at 60um (noise) f10d.fits Field N 300 at 100um f10dn.fits Field N 300 at 100um (noise) f11a.fits Field I 1613 at 12um f11an.fits Field I 1613 at 12um (noise) f11b.fits Field I 1613 at 25um f11bn.fits Field I 1613 at 25um (noise) f11c.fits Field I 1613 at 60um f11cn.fits Field I 1613 at 60um (noise) f11d.fits Field I 1613 at 100um f11dn.fits Field I 1613 at 100um (noise) f12a.fits Field M 33 at 12um f12an.fits Field M 33 at 12um (noise) f12b.fits Field M 33 at 25um f12bn.fits Field M 33 at 25um (noise) f12c.fits Field M 33 at 60um f12cn.fits Field M 33 at 60um (noise) f12d.fits Field M 33 at 100um f12dn.fits Field M 33 at 100um (noise) f13a.fits Field N 628 at 12um f13an.fits Field N 628 at 12um (noise) f13b.fits Field N 628 at 25um f13bn.fits Field N 628 at 25um (noise) f13c.fits Field N 628 at 60um f13cn.fits Field N 628 at 60um (noise) f13d.fits Field N 628 at 100um f13dn.fits Field N 628 at 100um (noise) f14a.fits Field N 660 at 12um f14an.fits Field N 660 at 12um (noise) f14b.fits Field N 660 at 25um f14bn.fits Field N 660 at 25um (noise) f14c.fits Field N 660 at 60um f14cn.fits Field N 660 at 60um (noise) f14d.fits Field N 660 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N 5907 at 60um (noise) f74d.fits Field N 5907 at 100um f74dn.fits Field N 5907 at 100um (noise) f75a.fits Field Draco at 12um f75an.fits Field Draco at 12um (noise) f75b.fits Field Draco at 25um f75bn.fits Field Draco at 25um (noise) f75c.fits Field Draco at 60um f75cn.fits Field Draco at 60um (noise) f75d.fits Field Draco at 100um f75dn.fits Field Draco at 100um (noise) f76a.fits Field N 6744 at 12um f76an.fits Field N 6744 at 12um (noise) f76b.fits Field N 6744 at 25um f76bn.fits Field N 6744 at 25um (noise) f76c.fits Field N 6744 at 60um f76cn.fits Field N 6744 at 60um (noise) f76d.fits Field N 6744 at 100um f76dn.fits Field N 6744 at 100um (noise) f77a.fits Field N 6822 at 12um f77an.fits Field N 6822 at 12um (noise) f77b.fits Field N 6822 at 25um f77bn.fits Field N 6822 at 25um (noise) f77c.fits Field N 6822 at 60um f77cn.fits Field N 6822 at 60um (noise) f77d.fits Field N 6822 at 100um f77dn.fits Field N 6822 at 100um (noise) f78a.fits Field N 6946 at 12um f78an.fits Field N 6946 at 12um (noise) f78b.fits Field N 6946 at 25um f78bn.fits Field N 6946 at 25um (noise) f78c.fits Field N 6946 at 60um f78cn.fits Field N 6946 at 60um (noise) f78d.fits Field N 6946 at 100um f78dn.fits Field N 6946 at 100um (noise) f79a.fits Field I 5201 at 12um f79an.fits Field I 5201 at 12um (noise) f79b.fits Field I 5201 at 25um f79bn.fits Field I 5201 at 25um (noise) f79c.fits Field I 5201 at 60um f79cn.fits Field I 5201 at 60um (noise) f79d.fits Field I 5201 at 100um f79dn.fits Field I 5201 at 100um (noise) f80a.fits Field N 7331 at 12um f80an.fits Field N 7331 at 12um (noise) f80b.fits Field N 7331 at 25um f80bn.fits Field N 7331 at 25um (noise) f80c.fits Field N 7331 at 60um f80cn.fits Field N 7331 at 60um (noise) f80d.fits Field N 7331 at 100um f80dn.fits Field N 7331 at 100um (noise) f81a.fits Field N 7640 at 12um f81an.fits Field N 7640 at 12um (noise) f81b.fits Field N 7640 at 25um f81bn.fits Field N 7640 at 25um (noise) f81c.fits Field N 7640 at 60um f81cn.fits Field N 7640 at 60um (noise) f81d.fits Field N 7640 at 100um f81dn.fits Field N 7640 at 100um (noise) f82a.fits Field N 7793 at 12um f82an.fits Field N 7793 at 12um (noise) f82b.fits Field N 7793 at 25um f82bn.fits Field N 7793 at 25um (noise) f82c.fits Field N 7793 at 60um f82cn.fits Field N 7793 at 60um (noise) f82d.fits Field N 7793 at 100um f82dn.fits Field N 7793 at 100um (noise) f83a.fits Field WLM at 12um f83an.fits Field WLM at 12um (noise) f83b.fits Field WLM at 25um f83bn.fits Field WLM at 25um (noise) f83c.fits Field WLM at 60um f83cn.fits Field WLM at 60um (noise) f83d.fits Field WLM at 100um f83dn.fits Field WLM at 100um (noise) Francois Ochsenbein CDS 1995 Jan 13 UNKNOWN UNKNOWN * The file "summary" was created at CDS from the FITS headers of the files, completed with the names of the galaxies. VII_109.xml A Catalogue of Rich Clusters of Galaxies 7110A VII/110A Rich Clusters of Galaxies A Catalogue of Rich Clusters of Galaxies G O Abell H G Corwin Jr. R P Olowin Astrophys. J. Suppl. Ser. 70 1 1989 1989ApJS...70....1A Clusters, galaxy Galaxy catalogs Nonstellar objects Surveys Positional data Magnitudes Fundamental catalog galaxies: clusters: general galaxies: distances and redshifts galaxies: structure This is an all-sky catalog of 4073 rich clusters of galaxies, each having at least 30 members within the magnitude range m_3 to m_3 + 2 (m_3 is the magnitude of the third brightest cluster member) and each with a nominal redshift less than 0.2. The southern data have been collected from a survey of UK 1.2 m Schmidt telescope IIIa-J plates and films and have been reduced to the systems defined by the northern data previously published by G.O. Abell. A revised northern catalog, including Bautz-Morgan types and redshifts where known, is also included.
Revised northern "Abell Catalog" ACO "Abell" number --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min DE- declination sign --- DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin BMtype cluster classification in the Bautz- Morgan system --- Count number of cluster members between m3 and m3+2, corrected for background ct RAh2000 right ascension (hours) (J2000) h RAm2000 right ascension (minutes) min DE-2000 declination sign --- DEd2000 declination (degrees) (J2000) deg DEm2000 declination (minutes) arcmin Xpos rectangular coordinates of the apparent cluster center, referred to the south-east (lower left) edge of the Palomar Sky Survey prints (x coordinate) mm Ypos same with above (y coordinate) mm GLON galactic longitude l2 deg GLAT galactic latitude b2 deg z cluster redshift from Struble and Rood (1987b) --- Rich richness, from Abell (1958) --- Dclass distance class, from Abell (1958) --- m10 red magnitude of the tenth brightest cluster member, from Abell (1958) mag Notes for "table4.dat" Notes for "table5.dat" Notes for "table6.dat" Prefix prefix to the "Abell" cluster number 'A' = for "Abell" number of rich clusters in "table4.dat" and "table6.dat" 'S' = for "Abell" number of supplementary clusters in "table5.dat" --- ACO "Abell" number --- Field the Southern Sky Survey Field number in which the cluster is located --- Notes Notes for tables 4-6 --- docu.doc Explanation of tables 3-6 Koichi Nakajima CDS 1994 Mar 14 UNKNOWN UNKNOWN * The files of notes were provided by courtesy of H.G.Corwin to H. Andernach; it was numbered A145 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" * In this revised version (VII/110A), the tables 7A, 7B and 7C of the paper are appended. The document file, tables 3, 4, 5 and 6 of the previous version (VII/110) have not been changed, except removing spaces between '+/-' signs and data, other than the rectangular coordinates in tables 4, 5, and 6. * In the tables 7A-7C archived here, following changes were made: A letter 'A' was added in front of the northern cluster number. The string 'ASnnnn' for a cluster name was changed to 'Snnnn'. All Abell cluster names are strictly mentioned in the format (A1,I4), e.g. 'A 12' also in the text. * 14-Mar-1994: First archived, Koichi Nakajima <nakajima@higashi.hit-u.ac.jp> (The date of the latest archiving, see the date of each file.) * 28-Oct-1995: Inserted zeroes between sign and values of Xcen/Ycen values in tables 4 and 5. VII_110A.xml The Second Reference Catalogue of bright galaxies (RC2) 7112 VII/112 RC2 Catalogue The Second Reference Catalogue of bright galaxies (RC2) G de Vaucouleurs A de Vaucouleurs H G Corwin Jr. University of Texas Press, Austin ??? ??? 1976 1976 VII/155 : "Third Reference Catalogue of bright galaxies" (RC3) by de Vaucouleurs G., de Vaucouleurs A., Corwin Jr. H.G., Buta R.J., Paturel G. and Fouque P. (1991), with 23022 galaxies Galaxy catalogs This standardized documentation file does not contain a complete description of the electronic version of the RC2 catalogue; please refer to the "doc.tex" file prepared by Theresa A. Nagy and Robert S. Hill.
The RC2 catalogue Name RC2 identification (NGC, IC, or anonymous) --- m_Name Component identification (A, B, C, etc.) number=1 A '.' indicates double or multiple objects where the data refers to the combined objects, but the classification is the brightest component. --- RAh Hours RA, 1950.0 h RAm Minutes RA, 1950.0 min DE- Sign Dec, 1950.0 --- DEd Degrees Dec, 1950.0 deg DEm Minutes Dec, 1950.0 arcmin GLON Galactic longitude deg SGLON Supergalactic longitude deg MType Revised morphological Type (Table 2)(9) --- Hubble Numerical Hubble Sequence Index T (Table 3)(9) --- n_Hubble Remark on Hubble Sequence Index number=8 The flag concerning the numerical Hubble type is 'P'=peculiar 'R'=note '$'=doubtful '*'=uncertain --- Plate Source of plate (Table 4)(9) --- r_MType Morphological type author code (Table 5)(9) --- Yerkes_1 Yerkes list 1 type and color classes number=6 see details about Yerkes color and class on doc.tex, Table 6 --- Byurkan Nuclear type in Byurkan system number=2 See details in doc.tex; nuclear type has the values 1 = no central condensation 2 = weak central condensation 3 = strong central condensation but no star-like image 4 = star-like nuclear image at short exposure but nebulous at long exposure 5 = star-like nuclear image even at long exposures. The additional n_Byurkan flag may also contain a second Byurkan type when two independent classifications are given. Otherwise, this flag contains the symbols: S = small nucleus * = uncertain $ = doubtful --- n_Byurkan Note on Byurkan nucleus type number=2 See details in doc.tex; nuclear type has the values 1 = no central condensation 2 = weak central condensation 3 = strong central condensation but no star-like image 4 = star-like nuclear image at short exposure but nebulous at long exposure 5 = star-like nuclear image even at long exposures. The additional n_Byurkan flag may also contain a second Byurkan type when two independent classifications are given. Otherwise, this flag contains the symbols: S = small nucleus * = uncertain $ = doubtful --- logD25 Major isophotal diameter, log(D_25) 0.1arcmin logR25 Ratio major to minor diameter, log(R_25) --- logD(0)25 Face-on major isophotal diameter 0.1arcmin logAe Effective aperture diameter, log(Ae) 0.1arcmin u_logAe '*'=uncertain, '$'=doubtful --- ID Object identifications number=9 See documentation file doc.tex --- precRAm Centennial precession in RA, minutes 0.01min/yr precDEm Centennial precession in DE, arcminutes 0.01arcmin/yr GLAT Galactic latitude deg SGLAT Supergalactic latitude deg DDOType David Dunlap Obs. (van den Bergh) type number=7 see details about van den Bergh type and classes in doc.tex, Table 7. --- DDOClass David Dunlap Obs. luminosity class number=7 see details about van den Bergh type and classes in doc.tex, Table 7. --- u_DDOClass '*'=uncertain, '$'=doubtful --- Weight Plate material weight number=9 See documentation file doc.tex --- Yerkes_2 Yerkes list 2 type and nuclear class number=6 see details about Yerkes color and class on doc.tex, Table 6 --- RC1 RC1 nuclear class number=9 See documentation file doc.tex --- e_logD25 Mean error of logD25 0.1arcmin e_logR25 Mean error of logR25 --- D0 Corrected log(D(0)25) for galactic extinc. 0.1arcmin e_logAe Mean error of log(Ae) 0.1arcmin Hmag Harvard photographic magnitude, mH mag u_Hmag if Hmag uncertain --- BT Total asymptotic B magnitude (BT) mag n_BT Flag on BT, see note number=3 The flag on BT or asymptotic colors has the following meaning: '*' if no total magnitude could be derived with single aperture observations requiring corrections in excess of 0.5 mag. 'S' if magnitude or color is a weighted mean. --- SuBr Mean B surface brightness within Ae number=9 See documentation file doc.tex mag/arcsec2 Extinct Galactic extinction in B system (A_B) number=9 See documentation file doc.tex mag (B-V)T Asymptotic color index number=9 See documentation file doc.tex mag n_(B-V)T Flag on (B-V)T, see comment number=3 The flag on BT or asymptotic colors has the following meaning: '*' if no total magnitude could be derived with single aperture observations requiring corrections in excess of 0.5 mag. 'S' if magnitude or color is a weighted mean. --- (U-B)T Asymptotic color index number=9 See documentation file doc.tex mag n_(U-B)T Flag on (U-B)T, see comment number=3 The flag on BT or asymptotic colors has the following meaning: '*' if no total magnitude could be derived with single aperture observations requiring corrections in excess of 0.5 mag. 'S' if magnitude or color is a weighted mean. --- (B-V)Ae Effective aperture color index number=9 See documentation file doc.tex mag n_(B-V)Ae Flag on (B-V)Ae, see comment number=3 The flag on BT or asymptotic colors has the following meaning: '*' if no total magnitude could be derived with single aperture observations requiring corrections in excess of 0.5 mag. 'S' if magnitude or color is a weighted mean. --- (U-B)Ae Effective aperture color index number=9 See documentation file doc.tex mag n_(U-B)Ae Flag on (U-B)Ae, see comment number=3 The flag on BT or asymptotic colors has the following meaning: '*' if no total magnitude could be derived with single aperture observations requiring corrections in excess of 0.5 mag. 'S' if magnitude or color is a weighted mean. --- B-V Total B-V color index, corrected number=9 See documentation file doc.tex mag logS_R Radio continuum flux near 1.4GHz (21cm) 10mJy n_logS_R Conditional code for logS_R number=4 the flag on logS has the approximate meaning (see doc.tex for details): '$' indicates discrepancies '*' indicates uncertainty '+' if a close pair was in the beam --- SpIndex1 Spectral index, {alpha}- for {nu} < {nu}_R --- u_SpIndex1 '*'=uncertain, '$'=very uncertain --- logS_H Integrated HI flux density 10-22W/m2 n_logS_H Conditional code for logS_H number=4 the flag on logS has the approximate meaning (see doc.tex for details): '$' indicates discrepancies '*' indicates uncertainty '+' if a close pair was in the beam --- RIndex Corrected radio index (RI) number=9 See documentation file doc.tex mag u_RIndex '$' for doubtful RIndex value --- RadVel Observed Radial velocity (cz) km/s u_RadVel '*' if discrepant RadVel values --- RadVel0 Radial velocity corrected for solar motion km/s Appendix Appendices codes, see comment number=5 indicates objects that have entries in the special appendices of the published catalogue: 'P': source of photographs in 18 atlases and major surveys; 'S': galaxies with supernovae; 'T': Hubble-Sandage and Hubble-Holmberg types. --- Zwicky Zwicky identifications --- HmagCorr Corrected Harvard photographic magnitude number=9 See documentation file doc.tex mag e_BT Estimated mean error of BT number=9 See documentation file doc.tex mag SuBrAv Average surface brightness number=9 See documentation file doc.tex mag/arcsec2 BT0 Corrected face-on magnitude number=9 See documentation file doc.tex mag e_(B-V)T Mean error of asymptotic color number=9 See documentation file doc.tex mag e_(U-B)T Mean error of asymptotic color number=9 See documentation file doc.tex mag e_(B-V)Ae Mean error of effective color number=9 See documentation file doc.tex mag e_(U-B)Ae Mean error of effective color number=9 See documentation file doc.tex mag (U-B)T0 Total corrected U-B color index number=9 See documentation file doc.tex --- o_SpIndex1 Number of radio continuum measurements --- o_logS_R Number of radio measurements for logS_R --- o_SpIndex2 Number of radio continuum measurements --- SpIndex2 Spectral index, {alpha}+ for {nu} > {nu}_R --- u_SpIndex2 '*'=uncertain, '$'=very uncertain --- o_logS_H Number of 21cm emission line observations --- A21 Self-absorption at 21 cm (1.4GHz) 0.4mag HI Neutral hydrogen index number=9 See documentation file doc.tex mag u_HI '$' if HI is doubtful --- o_RadVelR Number of radio observations for RadVel --- o_RadVelO Number of optical observations for RadVel --- e_RadVel Radial velocity mean error km/s DVelSun Solar motion correction, delta V km/s doc.tex Complete LaTeX documentation (needs adc.sty) Francois Ochsenbein CDS 1995 Sep 13 UNKNOWN UNKNOWN * See section 3 in "doc.tex" * available on the NASA "Selected Astronomical Catalogs" Vol. 1 CD-ROM, directory /nonstell/galaxies/rc2 * 13-Sep-1995 (CDS): compared to the CD-ROM version: - the decimal point was inserted when declination is given to the arcmin accuracy in file "catalog" - the document file "doc.tex" was corrected according to Harold Corwin's comments (except for units of radio fluxes) - the standardized "ReadMe" file was created VII_112.xml Catalogued Galaxies and Quasars observed in the IRAS Survey, Version 2 7113 VII/113 Cat Galaxies & QSOs observed in IRAS Survey, Vers.2 Catalogued Galaxies and Quasars observed in the IRAS Survey, Version 2 L Fullmer C J Londsdale JPL D-1932, Version 2, ??? ??? 1989 1989cgqo.book.....F Galaxy catalogs Infrared sources Photometry, infrared QSOs Surveys The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (<8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organization of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available. Notice: This file is NOT a complete scientific document for the catalogue; it serves only as a minimal description of the general format and structure of the data files. A copy of "Cataloged Galaxies and Quasars Observed in the IRAS Survey, 2" should be used to answer questions about the data in the IRAS Extragalactic Catalog.
Point source data IRASName Source name --- RAh Hours RA, equinox 1950.0, epoch 1983.5 h RAm Minutes RA, equinox 1950.0, epoch 1983.5 min RAs Seconds RA, equinox 1950.0, epoch 1983.5 s DE- Sign of DEC, equinox 1950.0, epoch 1983.5 --- DEd Degrees Dec, equinox 1950.0, epoch 1983.5 deg DEm Minutes Dec, equinox 1950.0, epoch 1983.5 arcmin DEs Seconds Dec, equinox 1950.0, epoch 1983.5 arcsec GLAT Galactic latitude deg UncMajor Uncertainty ellipse semi-major axis arcsec UncMinor Uncertainty ellipse semi-minor axis arcsec PosAng Uncertainty ellipse position angle measured East of North between the major axis of the ellipse and the local equatorial meridian. deg NHcon Number of times observed --- Fnu_12 Non-color corrected flux density at 12um Jy FQual_12 Flux quality at 12um number=1 Flux quality codes are (blank) = high quality; ':' = moderate quality; 'L' = upper limit --- Fnu_25 Non-color corrected flux density at 25um Jy FQual_25 Flux quality at 25um number=1 Flux quality codes are (blank) = high quality; ':' = moderate quality; 'L' = upper limit --- Fnu_60 Non-color corrected flux density at 60um Jy FQual_60 Flux quality at 60um number=1 Flux quality codes are (blank) = high quality; ':' = moderate quality; 'L' = upper limit --- Fnu_100 Non-color corrected flux density at 100um Jy FQual_100 Flux quality at 100um number=1 Flux quality codes are (blank) = high quality; ':' = moderate quality; 'L' = upper limit --- log(FIR) Decimal log of far infrared flux number=4 FIR estimates the flux that would have been measured within an ideal square bandpass 42.5-122.5um; it is a combination of 60 and 100 micron fluxes. See Appendix B, printed edition. W/m2 FQFIR FIR flux quality number=1 Flux quality codes are (blank) = high quality; ':' = moderate quality; 'L' = upper limit --- Relunc_12 Flux density uncertainty at 12um number=2 Uncertainties of FIR are coded as follows: A = from 0 to less than 4% B = from 4 to less than 8 C = from 8 to less than 12 D = from 12 to less than 16 E = from 16 to less than 20 F = equal to or greater than 20% --- Relunc_25 Flux density uncertainty at 25um number=2 Uncertainties of FIR are coded as follows: A = from 0 to less than 4% B = from 4 to less than 8 C = from 8 to less than 12 D = from 12 to less than 16 E = from 16 to less than 20 F = equal to or greater than 20% --- Relunc_60 Flux density uncertainty at 60um number=2 Uncertainties of FIR are coded as follows: A = from 0 to less than 4% B = from 4 to less than 8 C = from 8 to less than 12 D = from 12 to less than 16 E = from 16 to less than 20 F = equal to or greater than 20% --- Relunc_100 Flux density uncertainty at 100um number=2 Uncertainties of FIR are coded as follows: A = from 0 to less than 4% B = from 4 to less than 8 C = from 8 to less than 12 D = from 12 to less than 16 E = from 16 to less than 20 F = equal to or greater than 20% --- CC_12 Point source corr. coeff, 12um number=3 Correlation Coefficient codes are: A = 100%, B = 99%, C = 98%, ..., M = 88%, N = 87% --- CC_25 Point source corr. coeff, 25um number=3 Correlation Coefficient codes are: A = 100%, B = 99%, C = 98%, ..., M = 88%, N = 87% --- CC_60 Point source corr. coeff, 25um number=3 Correlation Coefficient codes are: A = 100%, B = 99%, C = 98%, ..., M = 88%, N = 87% --- CC_100 Point source corr. coeff, 100um number=3 Correlation Coefficient codes are: A = 100%, B = 99%, C = 98%, ..., M = 88%, N = 87% --- Cirr1 Number of nearby 100 micron only sources --- Cirr2 Ratio of cirrus flux to source flux --- Confuse Confusion flag, hex encoded number=5 Hex encoded flags compose the flags of the 4 passbands with masks 1=12um, 2=25um, 4=60um, 8=100um. See Table IV.A.1., printed edition. --- PNearH Number hours-confirmed point sources nearby If it exceeds 9, it is set equal to 9. --- PNearW Number weeks-confirmed point sources nearby If it exceeds 9, it is set equal to 9. --- HSDFlag High source density bin flag, hex encoded number=5 Hex encoded flags compose the flags of the 4 passbands with masks 1=12um, 2=25um, 4=60um, 8=100um. See Table IV.A.1., printed edition. --- SES1_12 Number of seconds-confirmed 12um SES (Small Extended Sources) nearby --- SES1_25 Number of seconds-confirmed 25um SES nearby --- SES1_60 Number of seconds-confirmed 60um SES nearby --- SES1_100 Number of seconds-confirmed 100um SES nearby --- SES2 Number of weeks-confirmed SES nearby hex encoded number=5 Hex encoded flags compose the flags of the 4 passbands with masks 1=12um, 2=25um, 4=60um, 8=100um. See Table IV.A.1., printed edition. --- NSSS Number of associations from SSS (Small Scale Structure) catalog --- SSSName Name of closest SSS association --- DisSSS Separation from the SSS source arcmin NonGal Number of associations from non-galaxy catalogs --- IdnGal Closest non-galaxy catalog association number=6 Codes for non-galaxy id's are in Table IV.A.2., printed edition. Very brief summary: ------------------------------------------------------------------------ 1 = SAO A = PN (Planetary Nebulae) 2 = HR (Bright Star) B = Parkes HII Survey 3 = DO (Dearborn Red *) C = Bonn HII Survey 4 = GCVS (Variable name) D = CO Velocities Toward HII Regions 5 = Wackerling (emission *) E = LDN (Lynds Dark Nebulae) 6 = NSV (Suspected Variables) F = AFGL (Air Force Geophys. Lab.) 7 = CCCS (Cool C*) G = IRC (2-um Sky Survey) 8 = Gliese (nearby *) H = EIC (Equatorial IR Catalogue) 9 = CSS (S*) I = IRC improved (Kleinmann+Joyce 1984) J = 1Jy (extragalactic sources) ------------------------------------------------------------------------ --- DSNGal Separation of the non-galaxy source arcmin NRecs Number of lines in "assoc.dat" file with IRAS name --- Association Data for Extragalactic Catalog IRASName IRAS source name --- PGCName Galaxy name from Primary Galaxy Catalog (UGC, UGCA, ESO, and CGCG) --- NPGC Number of appearances of PGCName in file --- DiamP Major axis diameter arcsec DisPGC Distance from IRAS source arcsec paPGC Position angle of separation vector measured in degrees East of North deg PosFlg Position flag number=1 The position and Magnitude flags are described in Section IX.A of the printed edition: B = The right ascension was changed to agree with the printed entry, or with a printed remark. C = The declination was changed to agree with the printed catalog. D = The position comes from the compilation of Dressel and Condon (1976). F = The right ascension was changed to agree with the conversion of printed galactic coordinates. G = The declination was changed to agree with the conversion of printed galactic coordinates. H = The magnitude was changed to agree with the printed version. K = The UGC and CGCG positions disagree, though the magnitudes agree. A combination of inspections of sky survey plates, UGC hardcopy notes, and cross-references using NGC or IC identifications resulted in the verification that the UGC and CGCG names refer to the same object. The UGC position has been adopted. L = As for K, but a better position than that given in either the UGC or CGCG was derived using a sky survey overlay, because neither of the catalogued positions was adequate. This new position should be accurate to about 1'. M = No CGCG object could be found that matched this UGC galaxy in position, although the UGC magnitude is not greater than 15.7. One possible explanation is that the galaxy is contained in one of the Zwicky lists of Selected Compact and Post-Eruptive Galaxies instead of the CGCG. N = A UGC and a CGCG galaxy are found with identical positions but the magnitudes disagree. The CGCG magnitude is brighter than the UGC magnitude by more than 1 magnitude. The UGC magnitude is quoted. P = As for N, except that the magnitudes disagree by less than 1 magnitude. The UGC magnitude is given. Q = The UGC and CGCG positions are identical, but the magnitudes disagree because the CGCG magnitude applies to individual members of a pair or group of galaxies, while the UGC magnitude applies to more than one of the members. The UGC magnitude is the one quoted. R = The UGC carries no magnitude so the CGCG magnitude is given. S = As for N, but the UGC magnitude is more than 1 magnitude brighter than the CGCG magnitude. The UGC magnitude is given. T = Similar case to Q except that the UGC and CGCG roles are reversed. The UGC magnitude is given. W = The magnitude listed here for each of the components of a galaxy group is the magnitude given the entire galaxy or galaxy group by the UGC. X = Combination of W and P. Z = The position was changed to agree with the CGCG position because the UGC position was found to be in error. --- MagFlg Magnitude flag number=1 The position and Magnitude flags are described in Section IX.A of the printed edition: B = The right ascension was changed to agree with the printed entry, or with a printed remark. C = The declination was changed to agree with the printed catalog. D = The position comes from the compilation of Dressel and Condon (1976). F = The right ascension was changed to agree with the conversion of printed galactic coordinates. G = The declination was changed to agree with the conversion of printed galactic coordinates. H = The magnitude was changed to agree with the printed version. K = The UGC and CGCG positions disagree, though the magnitudes agree. A combination of inspections of sky survey plates, UGC hardcopy notes, and cross-references using NGC or IC identifications resulted in the verification that the UGC and CGCG names refer to the same object. The UGC position has been adopted. L = As for K, but a better position than that given in either the UGC or CGCG was derived using a sky survey overlay, because neither of the catalogued positions was adequate. This new position should be accurate to about 1'. M = No CGCG object could be found that matched this UGC galaxy in position, although the UGC magnitude is not greater than 15.7. One possible explanation is that the galaxy is contained in one of the Zwicky lists of Selected Compact and Post-Eruptive Galaxies instead of the CGCG. N = A UGC and a CGCG galaxy are found with identical positions but the magnitudes disagree. The CGCG magnitude is brighter than the UGC magnitude by more than 1 magnitude. The UGC magnitude is quoted. P = As for N, except that the magnitudes disagree by less than 1 magnitude. The UGC magnitude is given. Q = The UGC and CGCG positions are identical, but the magnitudes disagree because the CGCG magnitude applies to individual members of a pair or group of galaxies, while the UGC magnitude applies to more than one of the members. The UGC magnitude is the one quoted. R = The UGC carries no magnitude so the CGCG magnitude is given. S = As for N, but the UGC magnitude is more than 1 magnitude brighter than the CGCG magnitude. The UGC magnitude is given. T = Similar case to Q except that the UGC and CGCG roles are reversed. The UGC magnitude is given. W = The magnitude listed here for each of the components of a galaxy group is the magnitude given the entire galaxy or galaxy group by the UGC. X = Combination of W and P. Z = The position was changed to agree with the CGCG position because the UGC position was found to be in error. --- MagPGC Magnitude from Primary Galaxy Catalog mag Class Classification --- MCG Morphological Catalog of Galaxies (MCG) number --- NMCG Number of appearances of MCG in file --- DiamMCG Major axis diameter arcsec DisMCG Distance from IRAS source measured in degrees East of North arcsec paMCG Position angle of separation vector deg NGCIC NGC or IC identification of Primary Catalog or MCG galaxy --- AMDName ARP, MKN, DDO associations --- NAMD Number of appearances of AMDName in file --- DisAMD Distance from IRAS source arcsec paAMD Position angle of separation vector measured in degrees East of North deg VVZName VCV (Veron-Cetty and Veron 1984), VV Verontsov-Velyaminov (Interact. Gal.), and Zwicky list associations --- NVVZ Number of appearances of VVZName in file --- DisVVZ Distance from IRAS source arcsec paVVZ Position angle of separation vector measured in degrees East of North deg VCVFlg VCV identifier or VV flag number=2 The flags relative to VV and VCV catalogues are described in Section IX.B of the printed edition: A = V10 has the same coordinates as V29 in the Atlas. The UGC name was used to confirm that the coordinate is correct for V29 and erroneous for V10. The UGC position for V10 = UGC 10814 was adopted. B = The V position is substantially different (>400") from positions for the object in other catalogs. The V position has been assumed to be in error because two or more other catalogs agree on a different position. The UGC position has been adopted. C = Same as for B, but the position from the Master List of Non-Stellar Sources (Dixon and Sonneborn 1980; the ML) has been adopted. D = The V position differs from that of the ML for the object. By use of overlays with the sky surveys, it has been established that the V position is in error so the ML position has been adopted. E = Same as for D, except that the ML position is not adequate either so a new position has been derived from the overlay which is accurate to about 1'. S1 = Seyfert type 1 galaxy. S2 = Seyfert type 2 galaxy. S3 = Seyfert type 3 galaxy, or "Liner". S or S? = Probably or possibly a Seyfert. H2 = Galaxy dominated by nuclear HII-regions, or "Starburst" nucleus. BL = BL Lac object. AN = "Active Nucleus". This flag is used when Veron-Cetty and Veron show no type for the object. --- RecNo Main Data Table record number for IRAS source --- intro.doc Excerpt from the published documentation Francois Ochsenbein CDS 1995 Jan 07 UNKNOWN UNKNOWN * From the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992) directory nonstell/galaxies/irasgal * 10-Jan-1995: set to blank the column 103 of file "xcat.dat" which contained the values 0, 1 or 2 (identical to the tens of RAh) for the records: # 1847 = IRAS 03216+7240 # 1952 = IRAS 03354+6633 # 2018 = IRAS 03434+6757 # 3437 = IRAS 07193+2211 # 4261 = IRAS 09065+5015 # 4325 = IRAS 09133+7431 # 5827 = IRAS 11463-6929 # 6278 = IRAS 12234+1315 # 7150 = IRAS 13317-4517 # 9810 = IRAS 19184-7404 #10378 = IRAS 21021+0927 #11367 = IRAS 23448+0139 The explanations of the flags PosFlg, MagFlg and VCVFlg have been added. VII_113.xml Massachusetts-Stony Brook Galactic Plane CO Survey. II. (l,V) maps of the first Galactic quadrant 7114 VII/114 Massachusetts-Stony Brook Galactic Plane CO Survey Massachusetts-Stony Brook Galactic Plane CO Survey. II. (l,V) maps of the first Galactic quadrant D P Clemens D B Sanders N Z Scoville P M Solomon ApJS 60, No. 1 297 1986 1986ApJS...60..297C Carbon monoxide Surveys The Massachusetts-Stony Brook Galactic Plane CO Survey data consisting of 40551 12CO J=1-0 spectra covering Galactic longitudes 8 - 90 deg and latitudes -1.05 - +1 deg, are presented. The spectra were obtained with the 14 m antenna at the Five College Radio Astronomy Observatory. Each spectrum consists of 350 channels with 1 km/s width; up to 300 channels per spectrum are defined. The extra channels allow for shifts of the central velocity with longitude to keep the Galactic emission within the frequency range of the backend. The spectra have RMS noise of 0.4 K per channel and intensities are on the T(R)* scale. The spectra were taken on a 3'x3' grid for longitudes between 18 deg and 55 deg. At other longitudes, the grid spacing was 6'x6'. The data are in 3-dimensional FITS files; the axes are LSR velocity, latitude, and longitude.
codata1.fit l = 8-17.9 deg codata2.fit l = 18-55 deg codata3.fit l = 55.1-89.9 deg Gail L. Schneider SSDOO/ADC Seth Digel SSDOO 1997 Aug 18 VII_114.xml Southern Galaxy Catalogue 7116 VII/116 Southern Galaxy Catalogue Southern Galaxy Catalogue H G Corwin Jr. A de Vaucouleurs G de Vaucouleurs The University of Texas Monographs in Astronomy No.4, The Department of Astronomy, University of Texas at Austin ??? ??? 1985 1985MAUTx...4....1C Galaxy catalogs (Abstract in the documentation file "docu") The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D>1.52.
notes for the catalogue GN galaxy name --- J plate number --- n_J 'r' denotes that a remark is given in "docu" file --- NOTE notes for the galaxy --- Koichi Nakajima CDS 1994 Jan 10 UNKNOWN UNKNOWN * The catalogue was provided by H. Andernach who took it out from NDADS/ARMS; it was numbered A110 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" * 10-Jan-1994: First archived. (The date of the latest archiving, see the date of each file.) VII_116.xml NGC 2000.0, The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters 7118 VII/118 NGC 2000.0 NGC 2000.0, The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters J L E Dreyer R W Sinnott Sky Publishing Corporation and Cambridge University Press ??? ??? 1988 1988QB853.D74...... Galaxy catalogs Nonstellar objects NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox B2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. The catalog lists object ID, object type, positions in equinox B2000.0, source of modern data (see NGC 2000 paperback copy), constellation, object size, magnitude, and the description of the object as given by Dreyer. The order of the new catalog is strictly by right ascension, the NGC and IC objects being merged into one machine-readable file. Copyright Notice: This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation.
The NGC 2000.0 Catalogue Name NGC or IC designation (preceded by I) --- Type Object classification the field is coded as follows: Gx Galaxy OC Open star cluster Gb Globular star cluster, usually in the Milky Way Galaxy Nb Bright emission or reflection nebula Pl Planetary nebula C+N Cluster associated with nebulosity Ast Asterism or group of a few stars Kt Knot or nebulous region in an external galaxy *** Triple star D* Double star * Single star ? Uncertain type or may not exist blank Unidentified at the place given, or type unknown - Object called nonexistent in the RNGC (Sulentic and Tifft 1973) PD Photographic plate defect --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin Source Source of entry sources that have been used to correct or update modern data in NGC 2000.0 (type, positions, magnitude, and size). Uppercase letters denote special NGC and IC errata lists, which have usually been accorded more weight than the source catalogues themselves. In parentheses after each citation is the number of times it has been used to update NGC entries (first number) and those in the IC (second number). A Archinal, Brent A. Version 4.0 of an unpublished list of errata to the RNGC, dated March 19, 1987. (110,0) a Arp, H., "Atlas of Peculiar Galaxies", 1966ApJS...14....1A (1,2) (Catalog <VII/74>) c Corwin, Harold G., Jr., A. de Vaucouleurs, and G. de Vaucouleurs, "Southern Galaxy Catalogue", Austin, Texas: University of Texas Monographs in Astronomy No. 4, 1985. (152,564) (Catalog <VII/116>) d Dreyer, J.L.E., New General Catalogue of Nebulae and Clusters of Stars (1888), Index Catalogue (1895), Second Index Catalogue (1908). London: Royal Astronomical Society, 1953. (28,2157) D Dreyer, J.L.E., ibid. Errata on pages 237, 281-283, and 366-378. (158,28) F Skiff, Brian, private communication of February 27, 1988. (93,36) h Holmberg, E., "A Study of Double and Multiple Galaxies", Lund Annals, 6, 1937. (13,2) k Karachentsev, I.D., "A Catalogue of Isolated Pairs of Galaxies in the Northern Hemisphere"; also, Karachentseva, V.E., "A Catalog of Isolated Galaxies." Astrofiz. Issled. Izv. Spetz. Astrofiz., 7, 3, 1972, and 8, 3, 1973. (0,4) (Catalogs <VII/77>, <VII/82>, <VII/83>) m Vorontsov-Velyaminov, B.A., and V.P. Arhipova, "Morphological Catalog of Galaxies", Parts I-V. Moscow: Moscow State University, 1962-74. (9,679) (Catalogs <VII/62> and <VII/100>) n Reinmuth, K., "Photographische Positionsbestimmung von NebelRecken" Veroff der Sternwarte zu Heidelberg, several papers, 1916-40. (0,4) o Alter, G., B. Balazs, and J. Ruprecht, Catalogue of Star Clusters and Associations, 2nd edition. Budapest: Akademiai Kiado, 1970. (5,0) (Catalogs <VII/5>, <VII/44> and <VII/101>) r Sulentic, Jack W., and William G. Tifft, "The Revised New General Catalogue of Nonstellar Astronomical Objects (RNGC)". Tucson, Arizona:University of Arizona Press, 1973. (4016,0) (Catalog <VII/1>) s Hirshfeld, Alan, and Roger W. Sinnott, eds., Sky Catalogue 2000.0, Vol.2, Cambridge, Massachusetts: Sky Publishing Corp. and Cambridge University Press, 1985. (3098,238) t Tully, R.B., "Nearby Galaxies Catalog". New York: Cambridge University Press, 1988. A preliminary version on magnetic tape (1981) was used here. (23,17) (Catalog <VII/145>) u Nilson P.N., Uppsala Ceneral Catalogue of Galaxies. Uppsala: Uppsala Astronomical Observatory, 1973. (15,543) (Catalog <VII/26>) v de Vaucouleurs, G., A. de Vaucouleurs, and H.C. Corvin, Jr., Second Reference Catalogue of Bright Galaxies. Austin, Texas, University of Texas Press, 1976.(118,206) (Catalog <VII/112>) x Dixon, R.S., and George Sonneborn, "A Master List of Nonstellar Optical Astronomical Objects (MOL)". Columbus, Ohio, Ohio State University Press, 1980. It should be noted that most of the information for codes a,h,k,m,n,o,u and z was extracted from the magnetic-tape version of this catalogue. The x code refers to IC objects identified in a literature search by these authors. (0,526) z Zwicky, F., E. Herzog, and P. Wild, "Catalogue of Galaxies and Clusters of Galaxies", Vol.I. Pasadena, Calif., California Institute of Technology, 1961. Also, successive volumes through 1968. (1,380) (Catalog <VII/49>) --- Const Constellation --- l_size Limit on Size --- size Largest dimension arcmin mag Integrated magnitude, visual or photographic (see n_mag) mag n_mag 'p' if mag is photographic (blue) --- Desc Description of the object description of the object, as given by Dreyer or corrected by him, in a coded or abbreviated form. The abbreviations and their combination are fully described in the introduction to the published catalog. ab about alm almost am among annul annular or ring nebula att attached b brighter bet between biN binuclear bn brightest to n side bs brightest to s side bp brightest to p side bf brightest to f side B bright c considerably chev chevelure co coarse, coarsely com cometic (cometary form) comp companion conn connected cont in contact C compressed Cl cluster d diameter def defined dif diffused diffic difficult dist distance, or distant D double e extremely, excessively ee most extremely er easily resolvable exc excentric E extended f following (eastward) F faint g gradually glob. globular gr group i irregular iF irregular figure inv involved, involving l little (adv.); long (adj.) L large m much m magnitude M middle, or in the middle n north neb nebula nebs nebulous neby nebulosity nf north following np north preceding ns north-south nr near N nucleus, or to a nucleus p preceding (westward) pf preceding-following p pretty (adv., before F. B. L, S) pg pretty gradually pm pretty much ps pretty suddenly plan planetary nebula (same as PN) prob probably P poor (sparse) in stars PN planetary nebula r resolvable (mottled, not resolved) rr partially resolved, some stars seen rrr well resolved, clearly consisting of stars R round RR exactly round Ri rich in stars s suddenly (abruptly) s south sf south following sp south preceding sc scattered sev several st stars (pl.) st 9... stars of 9th magnitude and fainter st 9..13 stars of mag. 9 to 13 stell stellar, pointlike susp suspected S small in angular size S* small (faint) star trap trapezium triangle triangle, forms a triangle with triN trinuclear v very vv _very_ var variable * a single star *10 a star of 10th magnitude *7-8 star of mag. 7 or 8 ** double star (same as D*) *** triple star ! remarkable !! very much so !!! a magnificent or otherwise interesting object --- Index of Messier and common names Object Common name (including Messier numbers) --- Name NGC or IC name, as in ngc2000.dat this field may be blank for Messier objects without NGC or IC counterparts. when one object corresponds to several entries in ngc2000, the Object is repeated (e.g. Copeland's Septet appears 7 times) --- Comment Text of comment, if any --- Francois Ochsenbein CDS 1997 Apr 03 Appreciation is expressed to William E. Shawcross for responding to a request from the ADC to make NGC 2000.0 available to the scientific community in machine-readable form. Mr. Shawcross also arranged for a copy of the machine-readable TEX file to be created for deposit in the archives of the data centers. I am grateful to both Mr. Shawcross and to Roger W. Sinnott for reviewing a draft copy of this document and making comments. The comments resulted in the finding and elimination of a few TEX symbols that were missed during the initial work. The meticulous documentation initiated by Wayne H. Warren at ADC (December 1989) is the basis of the present document. UNKNOWN UNKNOWN by Wayne H. Warren Jr., December 1989: It is important, even for users of the machine-readable catalog and this documentation, to also have a copy of the published book. In addition to the tables and reference sources mentioned in this document, the book provides an introductory section with a brief history of the NGC and IC catalogs, a count of objects by constellation, information on Dreyer's descriptions, a table cross index of Messier and NGC/IC designations, and a table of common names for NGC objects. The book also contains a table of right ascensions for NGC and IC objects. A magnetic tape containing NGC 2000.0 was received from William E. Shawcross of Sky Publishing Corporation on August 14, 1989. According to Mr. Shawcross, the file supplied to the ADC was an unmodified version of the one used to produce the book, and it still contained the TEX commands employed to produce the special symbols present in the printed version. As received, the file also contained a single copyright text record at its beginning. The text record was removed to an added first file in the archived version and supplemented with a small amount of additional information. The TEX in the data file was replaced by standard characters to represent the information. Special symbols, such as "\Delta", "\bigcirc", etc., were changed to their spelled-out equivalents. The size field was modified to add decimal points to integer numbers and to align all values properly so that the field can be processed with a single format specification. The magnitude field was modified by moving the "p" code for photographic magnitude to its own byte in order to remove it from the numerical field. Decimal points were added to all integer numbers in this field also. The catalog data file was run through the ADC General Verification Program, which checks data ranges and for various other problems that can be detected in a systematic way. Further history: The standardised document was generated in April 1977 at CDS (James Marcout, Francois Ochsenbein). VII_118.xml Catalogue of Principal Galaxies (PGC) 7119 VII/119 Catalogue of Principal Galaxies Catalogue of Principal Galaxies (PGC) G Paturel P Fouque L Bottinelli L Gouguenheim Astron. Astrophys. Suppl. Ser. 80 299 1989 1989A&AS...80..299P VII/137B : Third Reference Catalogue of bright galaxies (RC3) Galaxy catalogs This "catalog of principal galaxies" constitutes the basis of the "Third Reference Catalogue of Bright Galaxies" (RC3). It lists equatorial coordinates for the equinoxes 1950 and 2000 and cross identifications for 73197 galaxies. Of the 73197 galaxies, 40932 have coordinates with standard deviations of less than ten arcsec. Listed are 131,601 names from the 38 most common sources. These data are given when available: morphological descriptions, apparent major and minor axes, apparent magnitudes, radial velocities, and position angles.
The PGC catalogue PGC PGC Number number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- RAh Right Ascension 2000 (hours) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 h RAm Right Ascension 2000 (minutes) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 min RAs Right Ascension 2000 (seconds) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 s DE- Declination 2000 (sign) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- DEd Declination 2000 (degrees) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 deg DEm Declination 2000 (minutes) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 arcmin DEs Declination 2000 (seconds) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 arcsec RAh1950 Right Ascension 1950 (hours) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 h RAm1950 Right Ascension 1950 (minutes) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 min RAs1950 Right Ascension 1950 (seconds) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 s DE-1950 Declination 1950 (sign) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- DEd1950 Declination 1950 (degrees) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 deg DEm1950 Declination 1950 (minutes) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 arcmin DEs1950 Declination 1950 (seconds) number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 arcsec u_DEs An asterisk indicates coordinates with standard deviations less than 10arcsec number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- MType Morphological type class; see section 3.1 of the publication for details number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- MajAxis Major axis diameter at 25mag/arcsec2 number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 arcmin u_MajAxis Uncertainty (:?) or accuracy (*) flag on MajAxis number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- times separation character number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- MinAxis Minor axis diameter at 25mag/arcsec2 number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 arcmin u_MinAxis Uncertainty (:?) or accuracy (*) flag on MinAxis number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- Btot Apparent total magnitude; see section 3.3 of the publication for details number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 mag u_Btot An asterisk indicates magnitudes with accuracy less than 0.3mag number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- HRV Heliocentric Radial Velocity number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 km/s u_HRV An asterisk indicates velocities with standard deviations less than 30km/s number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- PA Position Angle from North eastward in 1950 frame number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 deg Name1 Name of galaxy in other sources number=2 acronyms and references for designations are given in Table 2 of the publication --- Name2 Name of galaxy in other sources number=2 acronyms and references for designations are given in Table 2 of the publication --- Name3 Name of galaxy in other sources number=2 acronyms and references for designations are given in Table 2 of the publication --- Name4 Name of galaxy in other sources number=2 acronyms and references for designations are given in Table 2 of the publication --- Cont if a continuation record exists number=1 field empty for continuation lines, i.e. preceding line has a '+' in byte 142 --- Francois Ochsenbein CDS 1995 Oct 03 UNKNOWN UNKNOWN * A copy of the catalogue on magnetic tape was provided to CDS by G. Paturel * 03-Oct-1995: description standardized at CDS VII_119.xml Catalog of SAS-2 Gamma-Ray Observations 7130 VII/130 SAS-2 Gamma-Ray Observations Catalog of SAS-2 Gamma-Ray Observations C E Fichtel R C Hartman S D Hunter D A Kniffen D J Thompson H B Oegelman M E Oezel Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center ??? ??? 1990 Gamma rays This catalog contains fluxes measured with the high-energy gamma-ray telescope flown aboard the second NASA Small Astronomy Satellite. The objects measured included various types of galaxies, QSOs, BL Lacertae objects, and pulsars. There are separate files for various types of objects, plus additional files for notes and references. The data cover about 60 percent of the sky and 89 percent of the galactic plane for gamma rays having energies >35 MeV. The data reported vary according to the types of objects. The galaxy file contains object designation and type, equatorial coordinates (B1950.0), 35-100 MeV emission limit, >100 MeV emission limit, and luminosity limit. The pulsar file contains object designation, period, period change (dP/dt), approximate distance, pulsed flux and luminosity limits, and notes. There is also a file containing data for miscellaneous other sources (SNRs, X-ray, and binary X-ray sources, etc.), but this file is not uniformly formatted because of its inhomogeneous data content.
This catalog summarizes final results for high-energy gamma-ray observations obtained with the second Small Astronomy Satellite (SAS-2) flown in an equatorial orbit by NASA from 1972 November through 1973 June. The data from the SAS-2 gamma-ray experiment cover about 60 percent of the sky and 89 percent of the galactic plane for gamma rays with energies >35 MeV. The experiment (also see Derdeyn et al. 1972) was a picture-type high-energy (>35 MeV) gamma-ray telescope using a 32-level wire-grid, magnetic-core spark chamber assembly covered by an anticoincidence scintillator and triggered by any one of four independent directional scintillator Cerenkov counter telescopes in anticoincidence with the outer scintillator. Thin tungsten (W) plates, 0.03 of a radiation length thick, were interleaved between the spark-chamber modules, which had an active area of approximately 640 sq cm. The large number of W plates and spark chambers served the dual purpose of providing material for the gamma rays to be converted to electron pairs that could then be clearly identified and from which their arrival directions could be determined; plus, they provided a means of ascertaining the energies of the electrons in a pair by measuring their Coulomb scattering. The full width at half-maximum field of view (FOV) was 35deg., and within the FOV the average angular uncertainty for determining the arrival direction of an individual gamma ray projected on one plane was about 2.6 deg. at 100 MeV and varied with energy approximately as E**1/2 in the energy range 35-200 MeV. For descriptions of the instrument calibration, data analysis procedures, and in-flight performance checks, see Fichtel et al. (1975) and Hartman et al. (1979). The primary sources for the data are Bignami et al. (1979), Fichtel et al. (1975, 1990), and Oegelman et al. (1976). SAS-2
Galaxy Data ID Object designation Common name or abbreviation for the observed object. --- Type Object type A letter code that designates the following object types: S Seyfert galaxy N N-type galaxy B BL Lacertae object Q Quasi-stellar object E Sharp emission-line galaxy O Other type of galaxy --- RAh Right ascension Equatorial coordinates - Decimal hours and degrees for equinox B1950.0. h DE- Sign of Declination --- DEd Declination deg EmLimit1 35-100 MeV emission limit Upper limits in the 35-100 MeV and >100 MeV energy ranges, as determined by using the diffuse gamma-ray emission level based on the analysis of Fichtel, Simpson, and Thompson (1978). These are 95% confidence upper limits calculated using the statistical analysis techniques of Hearn (1969), equations (12) and (13). keV/cm2/s EmLimit2 >100 MeV emission limit in photons/cm2/s photons/m2/s LumLimit Luminosity limit in units of ergs s-1 The 95% confidence upper limit to the gamma-ray luminosity for E >100 MeV. 0.1uW pulsar Data Pulsar Pulsar designation Standard pulsar coordinate designation (PSR) in hours and minutes of right ascension and degrees of declination. --- Period The pulsar period s Pchange Period change in units of 10-15 s s-1 Derivative of the period, which is the rate of pulsar spin up or spin down, in units of 10-5/s 10-15s/s Dist Distance The approximate distance of the object, as taken from Taylor and Manchester (1975). kpc FxLimit Pulsed flux limit in units of 10-6/cm2/s The 2-sigma. upper limit of the pulsed gamma-ray flux above 35 MeV in units of 10-6/sq cm/s. For most of the pulsars, this limit was calculated based on the highest single peak in the pulsar phase plot (see Oegelman et al. 1976 for details). 10-6/cm2/s LumLimit Luminosity limit in units of photon/s Upper limit to the gamma-ray luminosity, as determined from the upper limit to the flux and the distance estimates of Taylor and Manchester (1975). An emission solid angle of 1 steradian was assumed; the luminosity was calculated as: L = F*d**2 where F is the observed flux and d is the distance. Note that these upper limits do not truly reflect actual upper limits in the sense that neither the distance nor the emission solid angle is accurately known for any pulsar. photons/s note Notes and references (see pulsrnte.dat) Numerical key(s) to the notes and references given in file pulsrnte.dat, of the catalog. --- C.-H. Joseph Lyu & Paul Kuin Hughes STX/NASA 1997 Jan 27 UNKNOWN UNKNOWN The original ADC documentation by Wayne H. Warren (1990) was used to create this ReadMe file. The machine-readable galaxies and pulsars data files of the catalog were initially produced at the Astronomical Data Center from published papers supplied by Drs. Carl E. Fichtel and David L. Bertsch of the Laboratory for High Energy Astrophysics (LHEA) at the NASA Goddard Space Flight Center (GSFC), following a meeting with them in April 1988 that was arranged by Dr. J. M. Mead of GSFC. The newly created files were supplied to Dr. Stanley D. Hunter, also of the LHEA, who updated and added data to the existing files as well as creating the files for other sources. Further modifications were made in consultation with the above-mentioned authors. This document should be used only to supplement the information contained in the published papers. In addition to the primary source reference, those papers include Bigman et al. (1979), Fichtel et al. (1990), Fichtel et al. (1975), Thompson (1976), Lamb et al. (1977), Thompson et al. (1977a, 1977b, 1983), and Fichtel, Thompson, and Lamb (1987). VII_130.xml An Extragalactic Data Base II. The H I Data 7136 VII/136 Extragalactic Data Base II. The H I Data An Extragalactic Data Base II. The H I Data L Bottinelli L Gouguenheim P Fouque G Paturel A&AS 82 391 1990 1990A&AS...82..391B Galaxy catalogs H I data This catalog is a compilation of weighted mean H I parameters for 6439 galaxies. Raw 21-cm line widths have been reduced to a common system of widths at 20 and 50 percent of the peak intensity. They have been corrected for velocity resolution effects and tested for homogeneity. The H I fluxes, converted to uniform units, have been corrected for beam-filling effects. The catalog includes identification and alternate names, B1950 positions, line widths, H I flux, and heliocentric radial velocity. Details, including references to the original data, can be found in the published version.
Data PGC "PGC" --- ID PGC Number PGC Number according to the Catalogue of Principal Galaxies (Paturel et al., 1989 and 1989a) --- name Alternate Name priority: NGC, IC, UGC, ESO, MCG, UGCA, Mk, DDO, CGCG, Fairall, Arakelian, U.Michigan, Zwicky-compacts, VV, Arp, VCC, Weinberger, IRAS, KUG (see Paturel et al., 1989) --- RAh Right Ascension (1950) hours h RAm Right Ascension (1950) minutes min RAs Right Ascension (1950) seconds s DE- Declination (1950) sign --- DEd Declination (1950) degrees deg DEm Declination (1950) arcminutes arcmin DEs Declination (1950) arcseconds arcsec W20 21cm Line Width at 20% Weighted mean of 21cm line width at the level 20% of the peak. This width is corrected for velocity resolution. km/s e_W20 Standard Mean Error of W20 km/s W50 21cm Line Width at 50% Weighted mean of 21cm line width at the level 50% of the peak. This width is corrected for velocity resolution. km/s e_W50 Standard Mean Error of W20 km/s logS Log of Weighted Mean HI-Flux Log of the weighted mean HI-flux corrected for beam-filling effect. This flux and the associated error are both expressed in: log(10^-24 W*m^-2). --- e_logS Mean Error of logS --- RV Radial Velocity Weighted mean of the heliocentric radial velocity expressed in c*delta lambda/lambda. km/s e_RV Mean Error of RV km/s Julie Anne Watko SSDOO/ADC 1996 Feb 05 VII_136.xml CO Observations of Galaxies 1985-1989 7139 VII/139 Observations of Galaxies 1985-1989 CO Observations of Galaxies 1985-1989 F Verter Pub. Astron. Soc. Pacific 102 1281 1990 1990PASP..102.1281V VII/64 : Contains bibliography for 1985 and earlier data Abt, H. A. 1980, Pub. Astron. Soc. Pacific, 92, 249. Abt, H. A. 1985, Pub. Astron. Soc. Pacific, 97, 1050. Abt, H. A. 1990, preprint submitted to Pub. Astron. Soc. Pacific Baan, W. A., and Haschick, A. D. 1987, Astroph. J. 318, 139. Bell, M., and Seaquist, E. 1988, Astroph. J. 329, L17. Carlstrom, J. E. 1988, Ph.D. thesis, U. California at Berkeley de Boer, K. S., Azzopardi, M., Baschek, B., Dennefeld, M., Israel, F. P., Molaro, P., Seggewiss, W., Spite, F., and Westerlund, B. E. 1989, ESO Messenger, 57, 27. Gordon, M. A. 1990, Astroph. J. Let 350, L29. Harris, A. I., Wild, W., Stutzki, J., Jaffe, D. T., Jackson, J. M., Eckart, A., Lugten, J. B., and Genzel, R. 1989, Bull. Am. Astron. Soc. 21, 1188. Haynes, M. P., and Giovanelli, R. 1983, Astroph. J. 275, 472. Haynes, M. P., and Giovanelli, R. 1984, Astron. J. 89, 758. Henkel, C., Mauersberger, R., and Schilke, P. 1988, Astron. & Astrophy. 201, L23. Ho, P. T. P., Martin, R. N., Henkel, C., and Turner, J. L. 1987, Astroph. J. 320, 663. Israel, F. P. 1989, ESO Messenger, 57, 19. Israel, F. P., Hawarden, T. G., Wade, R., Geballe, T. R., and van Dishoeck, E. F. 1989, Mon. Notices Roy. Astron. Soc. 236, 89. Kenney, J. D., and Young, J. S. 1986, Astroph. J. Let. 301, L13. Kenney, J. D., and Young, J. S. 1988a, Astroph. J.sup 66, 261. Kenney, J. D., and Young, J. S. 1988b, Astroph. J. 326, 588. Kenney, J. D. P., and Young, J. S. 1989, Astroph. J. 344, 171. Mirabel, I. F., Kazes, I., and Sanders, D. B. 1988, Astroph. J. Let. 324, L59. Nguyen-Q-Rieu, Nakai, N., and Jackson, J. M. 1989, Astron. & Astrophy. 220, 57. Ohta, K., Sasaki, M., and Saito, M. 1988, Pub. Astron. Soc. Japan, 40, 653. Rickard, L. J, Palmer, P., Morris, M., Zuckerman, B., and Turner, B. E. 1975, Astroph. J. Let. 199, L75. Sandage, A., Binggeli, B., and Tammann, G. A. 1985, Astron. J. 90, 1759. Scoville, N. Z., Sanders, D. B., Sargent, A. I., Soifer, B. T., and Tinney, C. G. 1989, Astroph. J. Let. 345, L25. Stacey, G. J., Genzel, R., Lugten, J. B., and Townes, C. H. 1989, in The Physics and Chemistry of Interstellar Molecular Clouds, eds. G. Winnewisser and J. T. Armstrong (New York: Springer-Verlag) p.266 Verter, F. 1985, Astroph. J. Supp. 57, 261. Verter, F. 1987, Astroph. J. Supp. 65, 555. Verter, F. 1988, Astroph. J. Supp. 68, 129. Walker, C. E., Carlstrom, J. E., and Martin, R. N. 1989 Bull. Am. Astron. Soc.21, 1165. Wootten, A., and Schwab, F. R., eds., 1988, Science with a Millimeter Array, MMA Design Study Volume I, (Green Bank: NRAO). Young, J. S. 1990, in The Interstellar Medium in Galaxies, proc. Second Wyoming Conference, eds. H. A. Thronson Jr. and J. M. Shull (Dordrecht: Kluwer) p.67 Young, J. S., Xie, S., Kenney, J. D. P., and Rice, W. L. 1989, Astroph. J. Supp. 70, 699. Bibliography Galaxy catalogs Carbon monoxide References In this catalog a complete list of new publications which include CO observations of external galaxies has been edited so that new observations are reported only once, preferably in refereed journals (pub.dat). Therefore the catalog of publications also serves as an inventory of distinct observational projects. This catalog lists all publications that have appeared since the submission of Verter (1985) and before the end of 1989. For each publication, the number and nature of the observations are summarized.
This paper is a five year update to the Verter (1985) catalog of CO observations of galaxies. The goal of the present catalog is to give an overview of recent research on extragalactic molecular gas, as conducted through observations of emission from CO isotopes. This overview is intended to cover the number of galaxies observed, the nature of the observations, the number of individuals involved, the telescopes used, the degree of international, multi-observatory, and multi-wavelength collaboration, etc. The heart of the catalog is a complete inventory (Table 1) of research projects incorporating CO observations of galaxies which were published in 1985 - 1989, and a summary of their contents (Table 2). The Verter (1985) catalog contained all observations of CO isotopes in galaxies that were published, or available to the author in preprint form, prior to summer 1984. It contained data from 84 papers. The data were listed by individual galaxy; there were 94 galaxy detections and approximately 200 upper limits known at that time. The present catalog lists all published reports containing new observations of CO isotopes in galaxies that have appeared since the Verter (1985) catalog, through the end of 1989. This includes work which was incorporated in Verter (1985) in preprint form and was subsequently published. No preprints are included in the present catalog because it is too difficult to compile a complete listing of submitted work. This catalog contains 142 publications. The number of galaxies with CO detections is now approximately = 650, too large to list individually. Publication List: pub.dat is an alphabetical listing of the 142 publications containing observations of CO isotopes in galaxies. For each article, the reference and the title are provided. A comment in parentheses indicates those articles which were incorporated in Verter (1985) in preprint form. pub.dat was compiled with three goals: (1) to be as complete as possible in recording CO observations of galaxies, (2) to avoid repetition, and (3) to emphasize refereed publications. The completeness of the catalog is fairly easy to insure. Initially, pub.dat was developed over the past five years by perusing the literature on a regular basis and maintaining a list of articles that referred to molecular observations of galaxies. Finally, the completeness of the list was checked by going through the yearly indices of the refereed journals Ap. J., Astron. and Ap., A. J., M.N.R.A.S., and Pub. Astron. Soc. Japan}, as well as the subject index of Astronomy and Astrophysics Abstracts}. Preventing repetition of data in the catalog is a more difficult matter. The only insurance that the same data is not covered more than once is to read all of the articles and become familiar with their contents. In this manner it becomes obvious if the same observations were reported under different permutations of the authors' names or in different contexts. pub.dat only lists publications which present new observations, and does not include analyses of previously reported data. For example, pub.dat lists Verter (1987), which derives a luminosity function from reported observations, but does not list Verter (1988), which uses the same observations in a correlation study. Because of the preference for refereed journal articles, the following types of research reports appear in pub.dat only if they have not been superceeded by a refereed journal article on the same project: Ph.D. theses, conference proceedings, B.A.A.S. abstracts, articles in the ESO Messenger, etc. When non-refereed sources are cited, only one, preferably most recent, report will be listed for a given project. There is one set of exceptions to the above rules, made on behalf of the Five College Radio Astronomy Observatory (FCRAO) Extragalactic CO Survey. This survey is a multi-year effort to observe CO(1-0) emission in a large and complete sample of galaxies. The selection criteria are: all galaxies at declination above -20deg. with B(T) < 12 mag, or 100 microns IR flux density > 10 Jy, or 60 microns IR flux density > 5 Jy. The FCRAO Survey is by far the largest source of new galaxy detections in CO; by the beginning of 1990 about 270 galaxies had been observed, and about 2/3 of them detected (Young, private communication). Strictly speaking, these detections have been reported in one publication, Young etal. (1989). However, pub.dat lists almost all refereed publications which analyze subsets of this data, even though there is substantial overlap between their samples.
List of publications ref References to publications The name of the first author used in table2.dat is in brackets table2.dat summarizes the nature of the CO observations that are being taken by the various authors, and the telescopes which they used. --- Nature of Observations author Name of first author The alphabetical listing of publications is exactly the same as in pub.dat. The author's initials are only given if there is another person with the same last name who publishes in this field. --- N_author Total number of authors Includes the first author. --- note Note on number of authors An asterisk appears after two publications from the ESO Messenger; in these cases the complete list of collaborators does not appear on the by-line of the article, but is inferred from the text. --- year Year of publication yr obs Telescopes used (see table 1) --- trans Transistions measured Column five of table2.dat notes the CO transitions at which observations were taken. The number N indicates a rotational transition from level J = N to N-1. All observations are presumed to refer to the 12CO isotope, unless 13CO observations are indicated by the prefix ``13-". For papers that are primarily devoted to CO(1-0) data, observations of higher CO transitions and isotopes are only noted if they formed a significant element of the project. The term ``significant" was not applied strenuously, but indicates that the paper devoted more attention to the data at the higher transition than to merely mention it in passing. --- gal Number of galaxies observed The following notations are used to indicate various types of observations: N = N galaxies were detected (N) = N galaxies had upper limits N~M = N galaxies were detected at three of more points, as in a map. In counting the number of galaxies detected, interacting systems which overlap spatially were treated as one object. A listing of published CO maps of galaxies also appears in Young (1990), and is useful for looking up maps by galaxy name, although the listing is not complete. --- source Source selection For papers which are devoted to a few objects, their names are given; otherwise, the nature of the project or type of objects surveyed is described. Studies which are drawn from the data base of the FCRAO Extragalactic CO Survey are indicated by a leading (F). -------------------------------------------------------------------------------- TABLE 1: Telescopes Used in CO Observations of Galaxies ----------------------------------------------------------------------- observatory dish resolution abbrev. full name (m) 115GHz 230GHz ----------------------------------------------------------------------- BIMA Berkeley-Illinois-Maryland Array 6 x3 6" BTL AT&T Bell Laboratories 7 102" CSO CalTech Submillimeter Observatory 10.4 --- 30" ESO 3.6 European Southern Observatory 3.6 --- 60" FCRAO Five College Radio Astronomy Obs. 14 45" IRAM Institut Radio Astronomy Millimetrique 30 23" 14" JCMT James Clerk Maxwell Telescope 15 --- 23" NMA Nobeyama Millimeter Array 10 x5 6" NRAO National Radio Astronomy Observatory 12 60" 30" NRO Nobeyama Radio Observatory 45 17" OSO Onsala Space Observatory 20 33" OVRO Owens Valley Radio Observatory 10.4 x3 6" SEST Swedish-ESO Submillimetre Telescope 15 44" 23" S.mini Southern hemisphere twin of Columbia U. 1.2 480" "mini" telescope (original now at CfA) ----------------------------------------------------------------------- Table 1 defines the commonly used abbreviations for the observatories at which the data in this catalog were taken. For each observatory, columns one through five list its abbreviation, full name, antenna diameter, and the FWHM beam sizes at the rest frequencies of the CO(1-0) and CO(2-1) transitions. Beam sizes are only given for those transitions at which data from that telescope are reported in this catalog. It stands to reason that there must be a new, but growing, category of papers on molecular gas in external galaxies which contain no CO isotope data and thus go uncounted in this catalog. Some notable examples of this phenomenon are the recent work of Baan and Haschick (1987), Bell and Seaquist (1988), Carlstrom (1988), Henkel, Mauersberger, and Schilke (1988), Ho etal. (1987), Israel etal. 1989, Nguyen-Q-Rieu, Nakai, and Jackson (1989), Stacey etal. (1989), Walker, Carlstrom, and Martin (1989). As a consequence of the proliferation of accessible molecular lines, the past five year period is probably the last one in which a catalog of CO isotope observations can be used as a barometer of research on molecular gas in external galaxies. In order to continue to be useful, this catalog would have to be expanded to cover all molecular line observations, and since the effort required is prohibitive for one individual, the catalog will instead be discontinued. --- Nancy Grace Roman SSDOO/ADC 1996 Mar 01 Verter expresses thanks to Yoshiaki Taniguchi for providing a complete inventory of Nobeyama Radio Observatory Reports, and to Virginia Trimble and Harley Thronson for their comments on this paper. During the course of this work, that author was supported by a National Research Council Fellowship, and by NASA-ADP grants to proposals 074-89 and 092-89. The ADC wishes to thank Dr. Verter for forwarding this catalog and its to discussion. VII_139.xml Catalog of Galaxies Behind the Milky Way, l-210 to 230 degrees (Vol. 1) 7140 VII/140 Catalog of Galaxies Behind the Milky Way Catalog of Galaxies Behind the Milky Way, l-210 to 230 degrees (Vol. 1) M Saito H Ohtani A Asonuma N Kashikawa T Maki S Nishida T Watanabe Publ. Astron. Soc. Japan, Vol. 42 603 1990 1990PASJ...42..603S Catalog of Galaxies Behind the Milky Way, l-210 to 230 degrees (Vol. 1) M Saito H Ohtani A Baba N Hotta S Kameno S Kurosu K Nakada T Takata Publ. Astron. Soc. Japan, Vol. 43 449 1991 1991PASJ...43..449S Galaxy catalogs This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film ( 6.7 arcsec in size ) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of cataloged galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 ( Vol. 1 ) to that in 1989 ( Vol. 2 ), a surface brightness level deter- mining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper ( Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43 ). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito
l= 210 to 230 degrees l= 230 to 250 degrees num CGMW number --- field Field number of the ESO/SERC Southern Sky Survey --- X X coordinate on the film in millimeter --- Y Y coordinate on the film in millimeter --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin GLON Galactic longitude in degrees deg GLAT Galactic latitude in degrees deg majDiam Major diameter on the film in millimeter --- minDiam Minor diameter on the film in millimeter --- MType Morphological type class E: Elliptical I: Irregular S: Spiral SB: Barred Spiral --- feature Feature Bright, Faint: for surface brightness Asymm, Ring: for morphology Pair, Triple : for close association (If accompanying galaxies are almost in the same position, they are not listed in the catalog.) PN+galaxy : a foreground planetary nebula overlaps a galaxy --- Xident Cross identifications in other catalogs --- Gail L. Schneider, N.P.M. Kuin SSDOO/ADC 1995 Aug 04 UNKNOWN UNKNOWN The generation of machine-readable files and the data validation are carried out by the collaboration of authors and the Astronomical Data Analysis Center of the National Astronomical Observatory, Japan. Original Intro file: [ADAC/NAO] 22-Apr-1992 4-Aug-1995 [ADC] blanks between sign and number in several columns were replaced by zero's. VII_140.xml A Spectrophotometric Atlas of Galaxies 7141 VII/141 Spectrophotometric Atlas of Galaxies A Spectrophotometric Atlas of Galaxies R C Kennicutt Jr. ApJS 79 255 1992 1992ApJS...79..255K Galaxies, nearby Galaxies, spectra Spectrophotometry This catalog contains 56 spectra, the first are galaxy spectra, and the last is night sky spectrum. It is include for users wishing to check for low-level spurious features in the galaxy spectra. The spectra are intergrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength or 555 nm. This catalog can be used for a variety of applications but is not suitable for applications requiring precision colors over a long wavelength baseline such as computation of K-corrections, and some spectral synthesis applications. Tests show that the spectrophotometry in this catalog is accurate to the few percent level over small wavelength regions and is accurate to the 10-percent level over the entire wavelength range. Most observations cover the spectral range between 3650 and 7100 A with a resolution of 5 - 8 A.
Flux values for MK270 Flux values for MK3 Flux values for MK35 Flux values for MK487 Flux values for MK59 Flux values for MK71 Flux values for NGC1275 Flux values for NGC1357 Flux values for NGC1569 Flux values for NGC1832 Flux values for NGC2276 Flux values for NGC2775 Flux values for NGC2798 Flux values for NGC2903 Flux values for NGC3034 Flux values for NGC3077 Flux values for NGC3147 Flux values for NGC3227 Flux values for NGC3245 Flux values for NGC3303 Flux values for NGC3310 Flux values for NGC3368 Flux values for NGC3379 Flux values for NGC3471 Flux values for NGC3516 Flux values for NGC3623 Flux values for NGC3627 Flux values for NGC3690 Flux values for NGC3921 Flux values for NGC3941 Flux values for NGC4194 Flux values for NGC4262 Flux values for NGC4449 Flux values for NGC4472 Flux values for NGC4485 Flux values for NGC4631 Flux values for NGC4648 Flux values for NGC4670 Flux values for NGC4750 Flux values for NGC4775 Flux values for NGC4889 Flux values for NGC5195 Flux values for NGC5248 Flux values for NGC5548 Flux values for NGC5866 Flux values for NGC5996 Flux values for NGC6052 Flux values for NGC6181 Flux values for NGC6217 Flux values for NGC6240 Flux values for NGC6643 Flux values for NGC6764 Flux values for NGC7469 Flux values for NGC7714 Flux values for UGC6697 Flux values for night sky F(L)/F550 Normalized Flux at wavelength L L = 365.0+0.2*(I) nm; where I = sequence number of point with first point having I=0. NPTS=1726 Number of points in spectrum W(1)=3650 Wavelength of first data point in Angstroms DW=2 Wavelength increment in spectrum (Angstroms) VAR=F(LAMBDA)/F(5500) Normalization of fluxes (per unit wavelength) FORMAT=10F8.4 Formatting of flux data, in FORTRAN notation Each spectrum contain the 1726 flux values, ordered in wavelength as given above. Each line contains 10 points, with the exception of line 173, which contains 6 points. In some cases the original spectrum did not cover the entire 360-705-nm range, and at those wavelengths a data value of 0.0000 is listed. --- Gail L. Schneider SSDOO,ADC 1995 Feb 22 UNKNOWN UNKNOWN * Original description prepared by Dr. Robert C. Kennicutt, Jr., September 26, 1991 reformatted to CDS standard. VII_141.xml Southern Redshifts Catalogue and Plots 7142 VII/142 Southern Redshifts Catalogue Southern Redshifts Catalogue and Plots A P Fairall A Jones Publ. Dept. Astron., U. Cape Town No. 11 ??? ??? 1991 1991srcp.book.....F Galaxies, optical Redshifts This catalogue provides a "best-estimate" of the heliocentric radial velocities of some 13000 galaxies south of Declination 0 degrees. It is based on over 17000 redshift measurements, from over 200 sources, either published or otherwise made public. Aside from redshift references, each entry includes flags as to whether the velocity is from optical or radio observations, or both, as well as an indication of the nature of any optical emission lines. Galaxies with velocities beyond 75000 km/s are not included. All entries have been made interactivly, by one person (A.P.F.). The interaction was necessary because different investigators may use different names, quote slightly different positions, and obtain slightly different velocities for the same galaxy. Thus duplicate entries for the same galaxy are avoided (although a few may inevitably be included).
Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarilly lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilties and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.
The catalogue ID Designation The designations have been entirely picked up from the references quoted. Thus, if references choose to ignore recognised designations (such as NGC or ESO) they may also be absent in the catalogue. In general, ESO designations have been contracted to an "E" prefix. When multiple designations cause space problems, further contractions, such as NGC to an "N' prefix, are made. Further information to that given below is included, where appropriate, in the reference lists. --- RAh Right ascension hours, 1950.0 1950 Coordinates and galactic longitude and latitude are given. In earlier versions of the catalogue, declinations were rounded off to the nearest 15 arcsec - this remains for many entries under references 001 to 078. Some entries from Ref 131 onwards were entered from files (put in the same format as the Bologna catalogue); these have declinations rounded off to the nearest 6 arcsec. Where galaxies are reported by different observers, small differences in coordinates sometimes occur, but usually these are less than 3s in R.A. and 30 arecsec in Declination. In general, many observers make use of the Lauberts catalogue so positions are coincidental in the stated coordinates. h RAm Right ascension minutes, 1950.0 1950 Coordinates and galactic longitude and latitude are given. In earlier versions of the catalogue, declinations were rounded off to the nearest 15 arcsec - this remains for many entries under references 001 to 078. Some entries from Ref 131 onwards were entered from files (put in the same format as the Bologna catalogue); these have declinations rounded off to the nearest 6 arcsec. Where galaxies are reported by different observers, small differences in coordinates sometimes occur, but usually these are less than 3s in R.A. and 30 arecsec in Declination. In general, many observers make use of the Lauberts catalogue so positions are coincidental in the stated coordinates. min RAs Right ascension seconds, 1950.0 1950 Coordinates and galactic longitude and latitude are given. In earlier versions of the catalogue, declinations were rounded off to the nearest 15 arcsec - this remains for many entries under references 001 to 078. Some entries from Ref 131 onwards were entered from files (put in the same format as the Bologna catalogue); these have declinations rounded off to the nearest 6 arcsec. Where galaxies are reported by different observers, small differences in coordinates sometimes occur, but usually these are less than 3s in R.A. and 30 arecsec in Declination. In general, many observers make use of the Lauberts catalogue so positions are coincidental in the stated coordinates. s DE- Declination sign --- DEd Declination degrees, 1950.0 deg DEm Declination minutes, 1950.0 arcmin DEs Declination seconds, 1950.0 arcsec glon Galactic longitude deg glat Galactic latitude deg RV Velocity This column provides the "best estimate" of the Heliocentric velocity. If only a single reference is available, then the value quoted is straight from that reference. Although individual errors are not shown, a general error for the reference concerned may be shown in the reference list. The authors have tried to provide estimated EXTERNAL errors for the refences. Where these are not shown, one can assume the standard deviation of the external error to be in the region 100-120 km/s. As a general rule, the true external errors are twice that claimed by the authors! Experience has shown that, in general, about one or two percent of the redshift velocities from a given source are completely erroneous (and sometimes the percentage is higher). This is apparently unavoidable, given the nature of optical galaxy spectra or radio confusion, and even the most careful investigators are sometimes fooled by spurious features or detections. Similarly, cross correlations on optical spectra can sometimes latch on to the wrong values. Since the bulk of this catalogue concerns single reference redshifts, it is possible that 1 percent or so are erroneous. When two or more redshift references are shown for a galaxy, the catalogue velocity is a form of mean value, rounded off to the nearest 10 km/s (except if the velocities agreed to within 20 km/s, when it is rounded to 1 km/s). In deciding this mean value, extra weighting was given to certain references known to be more accurate. In general, those optical velocities from higher dispersion spectra (with external errors better than 50 km/s) had triple weight. Radio redshifts were given still higher weight, but only when supported by optical observations. If the reference numbers for an individual galaxy are not sequential (eg 132 076), then the mean value is weighed towards the value in the first reference (ie 132). The maximum acceptable differences between optical velocities is considered here to be 400 km/s, that between radio velocities is 100 km/s. If only two references are available, and there is no indication as to which is likely to be correct, then, rather than enter an uncertain value, a flag "LD" (for Large Difference) is substituted when the difference is greater than the above. Where there are three or more references, but one is discrepant (the others are considered valid), the discrepant reference is separated from the others by a blank space (e.g. 079 082 076). There are, in the catalogue, a few cases where three references fail to show any agreement, and one case where four different references all show totally different redshifts for the same galaxy. A few authors quote only galactocentric, rather than heliocentric, velocities, ie Vo (= V + 300 sin l cos b); where possible, we have calculated cz = V, but usually rounded off to 10 km km/s n_RV Velocity flag There are other cases where flags occur in place of a velocity. These are: SS - Superposed foreground star with near zero velocity. NE - No strong emission lines. The quality of the spectrogram did not permit redshift determination, but strong emission lines can be excluded. TF - Too faint. The galaxy is of low surface brightness and only a tentative redshift (not given) could be obtained, or no redshift obtained from the spectrogram. ESO4 - Reference 048. Observed spectroscopically at the European Southern Observatory, but no accurate redshift apparently yet available. NV - Observed spectroscopically but no velocity yet available. Worth including because of classification under Type column (e.g. Seyfert). --- ref1 Reference 1 The source references are given a three-digit numerical code. (See refs.dat.) As mentioned above, the catalogue was originally founded on data extracted from the de Vaucouleurs Second Reference Catalogue (Reference 001 - which covers redshift measurements published 1975 and earlier) with subsequent additions (References 002 onwards). Thus the listing that follows forms a source of southern redshifts, except that a number of Seyfert galaxies, having a single reference for a single galaxy, have been put under umbrella Seyfert lists. The numerical codes for references simply reflect the order in which the data were entered into the catalogue. It is roughly chronological (but occasionally a reference overlooked earlier is added). Gaps in sequential reference numbers result from some consolidation of references used in earlier editions. or where references are not yet public. When multiple references are listed, the order may reflect the weighting given to velocities (see above). --- ref2 Reference 2 The source references are given a three-digit numerical code. (See refs.dat.) As mentioned above, the catalogue was originally founded on data extracted from the de Vaucouleurs Second Reference Catalogue (Reference 001 - which covers redshift measurements published 1975 and earlier) with subsequent additions (References 002 onwards). Thus the listing that follows forms a source of southern redshifts, except that a number of Seyfert galaxies, having a single reference for a single galaxy, have been put under umbrella Seyfert lists. The numerical codes for references simply reflect the order in which the data were entered into the catalogue. It is roughly chronological (but occasionally a reference overlooked earlier is added). Gaps in sequential reference numbers result from some consolidation of references used in earlier editions. or where references are not yet public. When multiple references are listed, the order may reflect the weighting given to velocities (see above). --- ref3 Reference 3 The source references are given a three-digit numerical code. (See refs.dat.) As mentioned above, the catalogue was originally founded on data extracted from the de Vaucouleurs Second Reference Catalogue (Reference 001 - which covers redshift measurements published 1975 and earlier) with subsequent additions (References 002 onwards). Thus the listing that follows forms a source of southern redshifts, except that a number of Seyfert galaxies, having a single reference for a single galaxy, have been put under umbrella Seyfert lists. The numerical codes for references simply reflect the order in which the data were entered into the catalogue. It is roughly chronological (but occasionally a reference overlooked earlier is added). Gaps in sequential reference numbers result from some consolidation of references used in earlier editions. or where references are not yet public. When multiple references are listed, the order may reflect the weighting given to velocities (see above). --- ref4 Reference 4 The source references are given a three-digit numerical code. (See refs.dat.) As mentioned above, the catalogue was originally founded on data extracted from the de Vaucouleurs Second Reference Catalogue (Reference 001 - which covers redshift measurements published 1975 and earlier) with subsequent additions (References 002 onwards). Thus the listing that follows forms a source of southern redshifts, except that a number of Seyfert galaxies, having a single reference for a single galaxy, have been put under umbrella Seyfert lists. The numerical codes for references simply reflect the order in which the data were entered into the catalogue. It is roughly chronological (but occasionally a reference overlooked earlier is added). Gaps in sequential reference numbers result from some consolidation of references used in earlier editions. or where references are not yet public. When multiple references are listed, the order may reflect the weighting given to velocities (see above). --- ref5 Reference 5 The source references are given a three-digit numerical code. (See refs.dat.) As mentioned above, the catalogue was originally founded on data extracted from the de Vaucouleurs Second Reference Catalogue (Reference 001 - which covers redshift measurements published 1975 and earlier) with subsequent additions (References 002 onwards). Thus the listing that follows forms a source of southern redshifts, except that a number of Seyfert galaxies, having a single reference for a single galaxy, have been put under umbrella Seyfert lists. The numerical codes for references simply reflect the order in which the data were entered into the catalogue. It is roughly chronological (but occasionally a reference overlooked earlier is added). Gaps in sequential reference numbers result from some consolidation of references used in earlier editions. or where references are not yet public. When multiple references are listed, the order may reflect the weighting given to velocities (see above). --- ref6 Reference 6 The source references are given a three-digit numerical code. (See refs.dat.) As mentioned above, the catalogue was originally founded on data extracted from the de Vaucouleurs Second Reference Catalogue (Reference 001 - which covers redshift measurements published 1975 and earlier) with subsequent additions (References 002 onwards). Thus the listing that follows forms a source of southern redshifts, except that a number of Seyfert galaxies, having a single reference for a single galaxy, have been put under umbrella Seyfert lists. The numerical codes for references simply reflect the order in which the data were entered into the catalogue. It is roughly chronological (but occasionally a reference overlooked earlier is added). Gaps in sequential reference numbers result from some consolidation of references used in earlier editions. or where references are not yet public. When multiple references are listed, the order may reflect the weighting given to velocities (see above). --- type Type The second last column identifies Seyfert galaxies, and partially identifies other galaxies with emission lines in their optical spectra (where this can be easily read from the reference concerned). Abbreviations are as follows: S1 - Seyfert 1 S2 - Seyfert 2 S3 or S? - Suspected Seyfert BL - BL Lac object H2 - H II emission, generally implying strong emission lines of relatively high excitation, including [O III] 5007 + 4959 emission. EM - Generally implies low-excitation emission, [O II] 3727 and/or H-alpha, or unspecified emission. These classifications are obviously not uniform between different references, but nevertheless serve as a useful indication. --- flag Flag The flag is as follows: O - The reference or references only give optical velocities R - The reference or references only give radio velocities B - Both optical and radio velocities --- The references sorted alphabetically The references sorted by number ref Reference; the first line has a blank in byte 1, followed a 3-digit reference ID --- Nancy G. Roman ADC/SSDOO 1995 Jul 26 The authors thank. Penny Dobbie is thanked for help with layout and printing of the catalogue. They also thank various colleagues who have reported corrections to the previous version, particularly H. Winkler, H. Andernach, V. Liporetsky and G. Paturel. The Foundation for Research Development and University of Cape Town have provided research funding that contributed to the production of this work. The original document was prepared by the authors in October 1991. The contact for the first author is: Anthony P. Fairall, Department of Astronomy, University of Cape Town, Rondebosch. 7700 SOUTH AFRICA Telephone: (27)(21)650-2392 Fax: (27)(21)650-3726 E-mail: FAIRALL@UCTVAX.UCT.AC.ZA The document was prepared for the ADC by Anne C. Raugh and converted to the current standard form by the undersigned. The format tables were added. Various corrections were made to catalog.dat and the blank lines were removed from the reference tables. VII_142.xml Quasar Candidates from grens plates 7143 VII/143 Quasar Candidates Quasar Candidates from grens plates D Crampton D Schade A P Cowley Astron. J. 90 987 1985 1985AJ.....90..987C Quasar Candidates from grens plates D Crampton A P Cowley P C Schmidtke Astron. J. 96 816 1988 1988AJ.....96..816C Quasar Candidates from grens plates D Crampton A P Cowley F D A Hartwick Astron. J. 100 47 1990 1990AJ....100...47C VII/158 : Catalog of quasi-stellar objects (Hewitt & Burbidge, 1993) VII/188 : Quasars and Active Galactic Nuclei (7th Ed.) (Veron+ 1996) QSOs Redshifts This data set is based on data in three publications. The positions and magnitudes of quasar candidates discovered on Canada-France Hawaii-Telescope (CFHT) blue green plates are given. Spectroscopy with the Multiple Mirror Telescope (MMT) indicates that 70 percent of the candidates are quasars, and most of the others are white dwarfs or hot subluminous stars. Most of the redshifts are less than z=1.7. Additional spectroscopic observations at Steward Observatory were used. The catalog lists a name based on position, B1950 position, B magnitude, or visual magnitude, redshift, and remarks.
The catalogue Rem if there is a remark in the original catalogue --- Name Designation based on position --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Bmag B Magnitude, or visual estimate (cf n_Bmag) mag n_Bmag when Bmag is a visual estimate --- z Redshift (the last digit may be blank) --- u_z Uncertainty flag on z (* when z in unknown) --- Nature Remarks on the nature of the object --- Francois Ochsenbein CDS 1996 Nov 27 It is a pleasure to thank David Crampton <crampton@dao.nrc.ca> for providing the electronic data to M. Creze in October 1991, and for reviewing the initial version of the files. VII_143.xml Nearby Galaxies Catalogue 7145 VII/145 Nearby Galaxies Catalogue Nearby Galaxies Catalogue R B Tully Cambridge University Press ??? ??? 1988 1988QB857.T853..... Galaxy catalogs This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.
The Nearby Galaxies Catalog (NBG) Seq Running number --- Name Galaxy Name number=1 Entries are identified, in order of priority, by a NGC number (preceded by N), or by an UGC number (preceded by U), or by a name constructed from equatorial coordinates. See also other names in the four rightmost columns. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin HubCode Morphological type code number=2 the morphological type is given by a numeric code that is slightly different from RC2 one -5 E Elliptical -3 E/SO Elliptical/Lenticular (classification uncertain) -2 SO Lenticular 0 SO/a Lenticular/Spiral 1 Sa Spiral 2 Sab Spiral 3 Sb Spiral 4 Sbc Spiral 5 Sc Spiral 6 Scd Spiral 7 Sd Spiral 8 Sdm Spiral 9 Sm Spiral/irregular 10 Ir Irregular 12 S Spiral/irregular (classification uncertain) 13 P Peculiar Following the morphology number is a "B" (bar), "A" (absence of a bar), "X" (intermediate case), "P" (existence of a peculiarity) --- HubPec Morphological peculiarities number=2 the morphological type is given by a numeric code that is slightly different from RC2 one -5 E Elliptical -3 E/SO Elliptical/Lenticular (classification uncertain) -2 SO Lenticular 0 SO/a Lenticular/Spiral 1 Sa Spiral 2 Sab Spiral 3 Sb Spiral 4 Sbc Spiral 5 Sc Spiral 6 Scd Spiral 7 Sd Spiral 8 Sdm Spiral 9 Sm Spiral/irregular 10 Ir Irregular 12 S Spiral/irregular (classification uncertain) 13 P Peculiar Following the morphology number is a "B" (bar), "A" (absence of a bar), "X" (intermediate case), "P" (existence of a peculiarity) --- D25 Observed diameter at 25mag/arcsec2 isophote in blue number=3 Conversions from diameters in the major catalogues are: log(D25) = 0.983(D(UGC) + 0.3) - 0.051 log(D25) = 0.998(D(ESO) + 0.3) - 0.132 log(D25) = 1.020(D(MCG) + 0.3) - 0.007 arcmin D25bi Corrected diameter number=4 Diameter adjusted for effects of projection and obscuration. Adjustments are made according to the equation log(D25bi) = log(D25) - c log(D/d) + ABb.KD25, where D/d is the ratio of major to minor diameter c = 0.22 ABb is the Galactic (Milky Way) absorption in blue KD25 = 0.09 arcmin r_D25bi Reference for D25bi number=5 Source of diameter in decreasing order of priority 9 = standards (ref.12) 2 = UGC (ref.20) 6 = ESO (ref.16) 4 = MCG (ref.35) 5 = BCG (ref.7) 1 ** unspecified --- d/D Axial ratio of minor to major diameter --- i inclination from face-on number=6 The inclination is almost always given by i = 3deg + acos(sqrt(((d/D)^2 - 0.2^2)/(1 - 0.2^2))) deg BTbi Blue apparent magnitude adjusted for reddening number=7 BTbi is computed from: BTbi = BT - ABb - ABi0 mag r_BTbi Source for blue magnitudes number=8 Source of blue magnitudes in decreasing order of priority: 1 = Holmberg (ref.14) 2 = RC2 (ref.9) 7 = deVaucouleurs (ref.8) 6 = miscellaneous 3 = CGCG (ref.36) 5 = Harvard (ref.7) --- RadVel Heliocentric velocity km/s e_RadVel Mean error on RadVel km/s RefHI Reference to HI observation number=9 The telescopes used are NRAO 91m and 43m, the Max-Planck-Institut 100m and Parkes 64m, according to the following code: Code Telescope Resolution 1 91 22 km/s 2 43 22 3 91 5.5 4 43 5.5 5 100 5.5 6 100 22 7 64 4.9 --- V0 Systemic velocity (solar motion of 300km/s) km/s GLON Galactic longitude deg GLAT Galactic latitude deg SGLON Supergalactic longitude as in RC2 deg SGLAT Supergalactic latitude as in RC2 deg MB Absolute blue magnitude of galaxy mag m-M Distance modulus (5log(R)+25) mag R Distance, assuming H=75km/s/Mpc number=10 See also notes in the printed catalogue Mpc Delta25 Linear diameter (0.292 . D25bi * R) kpc SGX X coordinate in SuperGalactic frame Mpc SGY Y coordinate in SuperGalactic frame Mpc SGZ Z coordinate in SuperGalactic frame Mpc H-0.5bi Apparent magnitude at 1.6um adjusted for reddening number=10 See also notes in the printed catalogue mag B-H color (note: different apertures in B and H) mag ABi0 Obscuration within candidate galaxy number=10 See also notes in the printed catalogue mag ABb Obscuration within Milky Way mag W20 HI line width at 20% maximum number=10 See also notes in the printed catalogue km/s e_W20 Uncertainty on W20 km/s r_W20 Source for W20 number=11 Hydrogen line width and Flux literature references 2 R.J. Allen, B.F. Darchy, and R. Lauque, A&A 10,198, 1971. 3 R.J. Allen, W.M. Goss, R. Sancisi, W.T. Sullivan, III, and H. van Woerden. In "The Formahon and Dynamics of Galaxies", IAU Symposium, no. 58, ed. J.R. Shakeshaft, p.425. Dordrecht: Reidel, 1974. 5 C. Balkowski, L. Bottinelli, P. Chamaraux, L. Gouguenheim, and J. 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Robinson, and K.J. van Damme, Australian J. Physics, 19, 111, 1966. 67 B.J. Robinson, and J.A. Koehler, Nature, 208, 993, 1965. 69 D.H. Rogstad, I.A. Lockhard, and M.C.H. Wright, ApJ 193, 309, 1974. 72 D.H. Rogstad, and G.S. Shostak, A&A 22, 111, 1973. 76 R.R. Sholbrook, and B.J. Robinson, Australian J. Physics, 20, 131, 1967. 77 G.S. Shostak, ApJ 187, 19, 1974. 79 G.S. Shostak, ApJ 198, 527, 1975. 80 G.S. Shostak, and D.H. Rogstad, A&A 24, 405, 411, 1973. 96 E.E. Epstein, AJ 69, 490, 1964. 102 J.V. Hindman, F.J. Kerr, and R.X. McGee, Australian J. Physics, 16, 570, 1963. 105 L. Volders, and J.A. Hogbom, Bull. Astron. Inst. NL, 15, 307, 1961. 106 J. Heidmann, Bull. Astron. Inst. NL, 15, 314, 1961. 201 W.K. Huchtmeier, G.A. Tammann, and H.J. Wendker, A&A 46, 381, 1976. 202 W.K. Huchtmeier, G.A. Tammann, and H.J. Wendker, A&A 57, 313, 1977. 203 B. Balick, S.M. Faber, and J.S. Gallagher, ApJ 209, 710, 1976. 204 J.S. Gallagher, S.M. Faber, and B. Balick, ApJ 202, 7, 1976. 205 G.R. 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Salpeter, and N. Krumm, ApJS 46, 267, 1981. 301 K. Reif, U. Mebold, W.M. Goss, H. van Woerden, and B. Siegman, A&AS 50, 451, 1982. --- fH Flux correction factor number=12 All HI observations by the author and collaborators were single-beam measurements with a beam that is frequently smaller than the size of the source. The corrections are discussed in Ref.11 --- log(MH) mass of HI number=10 See also notes in the printed catalogue solMass log(MT) Total mass of Galaxy number=10 See also notes in the printed catalogue solMass MH/MT ratio of HI to total mass number=16 is sometimes larger than 1 due to the different methods for the computations of MH and MT --- log(LB) Intrinsic blue luminosity of galaxy number=10 See also notes in the printed catalogue Sun MH/LB ratio of HI to blue luminosity Sun MT/LB Mass to blue luminosity ratio Sun rho Density of galaxies number=13 density of galaxies brighter than -16mag in the vicinity of the entry. The local density was determined on a 3D-grid at 0.5Mpc spacing. See the details in the printed catalogue Mpc-3 Group Group affiliation number=14 galaxies may be affiliated with other galaxies in groups, associations, or clouds. The affiliations are described by a code in the form AB+/-CD+EF : a galaxy is located in cloud AB (see Note (1) in table "groups"), group -CD or first level association +CD, and second level association +EF. Galaxies are ordered by group in table "groups.dat" --- UGC/ESO Designation in UGC (number <= 12921) or ESO --- MCG designation in MCG (Ref. 35) --- inRC2 '2' when the galaxy in RC2 (ref. 9) --- OtherNames Other names separated by a comma number=15 The alternative names are that date back before 1976 can be found in BGC (ref.7) and RC2 (ref.9). More recent sources are designated Arak = Arakelian (ref. 3) CVndw = Lo and Sargent (ref.18) Kar = Karachentseva (ref.15) M81dw = Lo and Sargent (ref.18) RMB = Rubin et al. (ref.24) SAGDIG = Cesarsky et al. (ref. 5) SCLDIG = Laustsen et al. (ref.17) Scl = Rubin et al. (ref.23) Turn = Turner (ref.32) UGCA = Nilson (ref.21) UKS = Longmore et al. (ref.19) At the very end of this column there may be a notation that indicates if the galaxy has a Seyfert(S) or LINER(L) active nucleus; the number that follows specifies whether the type is 1, or 2, or an intermediate case. --- *Lists by groups Group Group identification number=1 the first two digits designate the Cloud, as follows: 11=Virgo Cluster and Southern Extension 12=Ursa Major Cloud 13=Ursa Major Southern Spur 14=Coma - Sculptor Cloud 15=Leo Spur 16=Centaurus Spur 17=Triangulum Spur 18=Perseus Cloud 19=Pavo - Ara Cloud 21=Leo Cloud 22=Crater Cloud 23=Centaurus Cloud 24=Lynx Cloud 31=Antlia - Hydra Cloud 32=Cancer - Leo Cloud 33=Carina Cloud 34=Lepus Cloud 41=Virgo - Libra Cloud 42=Canes Venatici - Camelopardalis Cloud 43=Canes Venatici Spur 44=Draco Cloud 45=Coma Cloud 51=Fornax Cluster and Eridanus Cloud 52=Cetus - Aries Cloud 53=Dorado Cloud 54=Antlia Cloud 55=Apus Cloud 61=Telescopium - Grus Cloud 62=Pavo - Indus Spur 63=Pisces - Austrinus Spur 64=Pegasus Cloud 65=Pegasus Spur 66=Sagittarius Cloud 71=Serpens Cloud 72=Bootes Cloud 73=Ophiuchus Cloud Other (multiple of 10) are Isolated groups. --- Name Galaxy name, as in catalog --- HubCode Morphological type code --- HubBar --- MB Absolute blue magnitude of galaxy mag MWay flag for our Galaxy --- V0 Systemic velocity km/s Identification of Rich clusters SuperCl Complex/Supercluster designation number=1 the notation is A.B, where A designates a complex, and A.B the Supercluster, as follows: 1 PISCES - CETUS SUPERCLUSTER COMPLEX 1.1 Pisces - Cetus Supercluster 1.2 Perseus - Pegasus Chain 1.3 Pegasus - Pisces Chain 1.4 Sculptor Region 1.5 Virgo - Hydra - Centaurus Supercluster 2 AQUARIUS SUPERCLUSTER COMPLEX 2.1 Aquarius - Capricornus Region 2.2 Aquarius Region 3 HERCULES - CORONA BOREALIS SUPERCLUSTER COMPLEX 3.1 Hercules Supercluster 3.2 Bootes Supercluster 3.3 Corona Borealis Supercluster 3.4 Corona Borealis - Hercules Supercluster 4 LEO SUPERCLUSTER COMPLEX 4.1 Leo Supercluster 4.2 Leo - Coma Supercluster 4.3 Sextans Supercluster 5 URSA MAJOR SUPERCLUSTER COMPLEX 5.1 Ursa Major Supercluster 5.2 Draco Supercluster --- Flag See Note number=2 the '*' indicates the cluster is in a sufficiently dense region in the core of the complex that a pathway can be found to every other cluster with an '*' in the same complex with cluster-to-cluster steps of less than 40Mpc. The '+' designates associations with the incompletely surveyed Indus region. --- Cluster designation (Abell or Anonymous) --- z Redshift --- SGX X coordinate in SuperGalactic frame Mpc SGY Y coordinate in SuperGalactic frame Mpc SGZ Z coordinate in SuperGalactic frame Mpc Francois Ochsenbein CDS 1994 Jul 20 UNKNOWN UNKNOWN * The original files were received from ADC/Greenbelt in 1994 as 3 data files tully.data1, tully.data2 and tully.data3, and a Fortran program tully.software to read the parameters of a galaxy which are on three lines in the file tully.data3 * 04-Jul-1995: data files converted to standard tables. A control character \001 in record#2168 (2119-45) has been removed, and the ReadMe file was generated. VII_145.xml Structure Parameters of galactic Globular Clusters 7151 VII/151 Structure Parameters of Galactic Globular Clusters Structure Parameters of galactic Globular Clusters R F Webbink IAU Symp 113 "Dynamics of Star Clusters", Ed. J. Goedman & P. Hut, 541 ??? ??? 1985 1985IAUS..113..541W VII/13 : Globular Cluster Catalogue (Arp 1965) Clusters, globular Magnitudes This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, & table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, & table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.
Observed Galactic Clusters Observed Galactic Dwarf Spheroidals Observed Fornax Globular Clusters IAU Cluster designation --- Name1 Cluster name --- Name2 Cluster name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination 1950 sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin VHB Apparent level of the cluster horizontal branch mag u_VHB Uncertainty flag (:) on VHB --- m_VHB Method used for the determination of VHB number=1 the method is coded as follows: CM = color-magnitude diagram (+/- 0.05) RR = mean magnitudes of RR Lyr variable (+/- 0.1) BG = magnitudes of the brightest giants (+/- 0.3) IR = combination of the index of richness, integrated apparent magnitude, estimated foreground reddening (+/- 0.6) A = foreground reddening plus assumed reddening law (+/- 1.4) --- r_VHB Reference of VHB determination --- l_EBV Limit flag for EBV --- EBV Color excess E(B-V) mag u_EBV Uncertainty flag (:) on EBV --- m_EBV Method used for the determination of EBV number=2 the method is coded as follows: HB = two-color diagram of blue horizontal branch (HB) stars NB = narrow-band photometry and spectroscopy of HB stars fit to model atmospheres B = color-magnitude diagram of blue HB stars fit to a fiducial curve rr = Sturch's method using RR Lyr colors at minimum RR = mean RR Lyr colors psi = slope of red continuum of individual giants DU = correlation of UV excesses of giant stars UB = asymptotic reddening of foreground stars in UBV uy = asymptotic reddening of foreground stars in uvby XY = asymptotic reddening of foreground stars in Vilnius photometry GB = blue edge of RR Lyr gap RD = red edge of RR Lyr gap CS = integrated optical or near-UV colors IR = integrated IR colors MI = correlation of metallicity index with integrated color HI = neutral Hydrogen column density plus galaxy counts CX = modified cosecant law --- r_EBV Reference for EBV determination --- BVg observed color of the cluster subgiant branch mag u_BVg Uncertainty flag (:) on BVg --- m_BVg Method for the determination of BVg number=3 the method is coded as follows: CM = color-magnitude diagram DP = period difference of RR Lyr variables DS = cluster metallicity in individual RR Lyr UB = integrated UBV colors Q = line blanketing index from integrated narrow-band photometry BV = integrated BV colors --- r_BVg Reference for BVg determination --- lgtt log(radius) expressed in arcmin arcmin u_lgtt Uncertainty flag (:) on lgtt --- m_lgtt Method for the determination of lgtt number=4 the method is coded as follows: SC = star counts SP = surface photometry AP = concentric aperture photometry D = correlation of apparent diameter with limiting radius e = eye estimate of the corde radius --- r_lgtt Reference for lgtt determination --- lgtc log(core radius) expressed in arcmin arcmin u_lgtc Uncertainty flag (:) on lgtc --- m_lgtc Method for the determination of lgtc number=4 the method is coded as follows: SC = star counts SP = surface photometry AP = concentric aperture photometry D = correlation of apparent diameter with limiting radius e = eye estimate of the corde radius --- r_lgtc Reference for lgtc determination --- eps Ellipticity number=5 the ellipticity only exists for table1b; methods and references for its determination are identical to the radius determinations lgtt and lgtc --- Vt Integrated V magnitude mag u_Vt Uncertainty flag (: or )) on Vt --- m_Vt Method for the determination of Vt number=6 the method is coded as follows: AP = concentric aperture photometry SP = surface photometry Sig = summation R = fit of the upper end of LF IR = index of richness --- r_Vt Reference for Vt determination --- l_Sc Limit flag for Sc --- Sc Central surface brightness mag/arcmin2 u_Sc Uncertainty flag (: or )) on Sc --- m_Sc Method for the determination of Vt and Sc number=6 the method is coded as follows: AP = concentric aperture photometry SP = surface photometry Sig = summation R = fit of the upper end of LF IR = index of richness --- r_Sc Reference for the determination of Vt and Sc --- Derived Galactic Clusters Derived Galactic Dwarf Spheroidals Derived Fornax Globular Clusters IAU Cluster designation --- Name1 Cluster name --- Name2 Cluster name --- GLON Galactic longitude deg GLAT Galactic latitude deg Rdist Heliocentric distance kpc Xdist Galactocentric distance kpc Ydist Galactocentric distance kpc Zdist Galactocentric distance kpc rGC Galactocentric distance kpc l_[m/H] Limit on [m/H] --- [m/H] log(metallicity) relative to Sun Sun Mv Integrated absolute magnitude of the cluster mag l_rc Limit flag on rc --- rc Core radius pc rt Limiting radius pc c Core Concentration parameter = log(rt/rc) --- l_lg.tr Limit flag on lg.tr --- lg.tr log of central relaxation time (yr) yr l_lg.rho Limit flag on lg.rho --- lg.rho log of central mass density (solar masses per cubic parsec) solMass/pc3 l_s0 Limit flag on s0 --- s0 Central velocity dispersion km/s l_Vesc Limit flag on Vesc --- Vesc Central escape velocity km/s Francois Ochsenbein CDS 1996 Aug 22 UNKNOWN UNKNOWN * 12-Jan-1993: The catalogue was prepared at CDS (M.J. Wagner) from the printed catalogue. * 22-Aug-1996: Documentation and files converted to CDS Standards VII_151.xml Third Reference Catalogue of Bright Galaxies (RC3) 7155 VII/155 Third Reference Cat. of Bright Galaxies Third Reference Catalogue of Bright Galaxies (RC3) G de Vaucouleurs A de Vaucouleurs H G Corwin Jr. R J Buta G Paturel P Fouque Springer-Verlag: New York, ??? ??? 1991 1991trcb.book.....D VII/112 : RC2 Catalogue VII/119 : PGC Catalogue (Paturel et al., =1989A&AS...80..299P) J/AJ/108/2128 : RC3 corrections & additions Galaxy catalogs The University of Texas has revised its third edition of its catalogue of bright galaxies. This not only contains many more entries than the second edition (23,022) but substantially more information for each entry.
The original Harvard Survey of the External Galaxies brighter than the 13th magnitude, by H. Shapley and A. Ames (1932), included just 1,249 objects (of which five were not galaxies), with estimated photographic magnitudes and diameters from heterogeneous sources. The first Reference Catalogue of Bright Galaxies (RC1) (G. and A. de Vaucouleurs 1964), prepared between 1949 and 1963, included 2,599 objects (six are not galaxies), over twice the number in the original Shapley-Ames catalogue. In addition to diameters, magnitudes, colors, and redshifts in relatively homogeneous systems, it gave revised classifications and detailed literature references from 1913 to 1963. (NGC 8 is a double star; NGC 4361 is a planetary nebula; NGC 5396 is nonexistent, probably = NGC 5375; IC 1308 is a H II region in NGC 6822; IC 3917 is nonexistent, probably a plate defect (M. Wolf 1905); and A2144 = Palomar 12 is a globular cluster.) The Second Reference Catalogue (RC2) (G. and A. de Vaucouleurs, and H. G. Corwin 1976), prepared between 1971 and 1975, included 4,364 objects (two are not galaxies), for which it gave improved isophotal diameters and axis ratios in the D25 system, newly determined total magnitudes and colors in the UBV system, continuum and 21-cm radio magnitudes, HI index, and redshifts, as well as references to published photographs and a bibliography for the years 1964 to 1975. Both the First and Second Reference Catalogues are limited to galaxies with useful literature references and are incomplete beyond the Shapley-Ames limit. (A0733+02 = DDO 45 is a planetary nebula; A2143-21 = Palomar 12 is a globular cluster.) The present, much enlarged Third Reference Catalogue of Bright Galaxies (RC3) attempts to be reasonably complete for galaxies having apparent diameters larger than 1 arcmin at the D25 isophotal level and total B-band magnitudes BT brighter than about 15.5, with a redshift not in excess of 15,000 km/s. Objects of special interest, such as compact galaxies smaller than 1 arcmin or fainter than magnitude 15.5, and those already in RC2, are also included. The number of RC3 objects meeting these conditions is 11,897. Additional objects meeting only the diameter or the magnitude condition, and objects of interest smaller than 1.00, fainter than 15.5, or with redshifts > 15,000 km/s, bring the total to 23,022. (PGC 41636 and P65386 have been deleted since the catalogue was printed. The first is a globular cluster, Palomar 15, and the second is a duplicate entry for NGC 6967.) These were extracted from the database of 73,197 galaxies maintained by G. Paturel at Lyons Observatory (Paturel et al. 1989a,b). Data published prior to mid-1990 are included in the main RC3 table and appendices. As might be expected in a compilation of this size, a number of errors have been detected since this catalog was archived. These have been corrected by H. G. Corwin who submitted the current, corrected version. Any problems relating to the catalogue itself should be addressed to him: Dr. Harold G. Corwin, Jr. IPAC, M/S 100-22 California Institute of Technology Pasadena, CA 91125 Details of the reduction procedures, and Notes, References, and Appendices are in Volume 1 of the printed version of RC3, available from Springer-Verlag New York. Volumes 2 and 3 (included in this distribution) are also be available from Springer-Verlag should you wish to have a printed and bound version of the complete catalogue. The user of this catalogue is referred to this source volume for notes, references to data on individual galaxies, and the important information contained in the appendices as well as a discussion of how the entries were derived. We ask that you acknowledge RC3 and its authors in any publication that results from your use of the Catalogue. You may also freely distribute unaltered electromagnetic copies of RC3 to friends and colleagues as long as a copy of this documentation - including this notice - accompanies the Catalogue. The printed version of RC3 is protected by copyright, and may not be reproduced in any manner without the written permission of the copyright holder, Springer-Verlag New York, Inc.
The revised RC3 catalog RAh Right Ascension 2000 (hours) The right ascensions and declinations for the equinox 2000.0, are precessed from the 1950.0 position using the 1976 IAU constants (see, e.g., the Supplement to The Astronomical Almanac for 1984). These are given to 0.1 second of time and 1 arcsec when available, and to 0.1 minute of time and 1 arcmin otherwise (Section 3.1.a, page 11). The right ascensions originally given with an accuracy of 0.1min have been converted to seconds; such converted RAs and RAs1950 values have no decimal, and the corresponding DEs and DEs1950 are blank. h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (sec. or min.) s DE- Sign of declination --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec RAh1950 Right Ascension 1950 (hours) h RAm1950 Right Ascension 1950 (minutes) min RAs1950 Right Ascension 1950 (sec. or min.) s DE-1950 Sign of declination 1950 --- DEd1950 Declination 1950 (degrees) deg DEm1950 Declination 1950 (minutes) arcmin DEs1950 Declination 1950 (seconds) arcsec GLON Galactic longitude The galactic coordinates given to 0.01, are calculated following the IAU 1958 prescription (Blaauw et al. 1960) with the North Galactic Pole at alpha = 12h49m , delta = +27 24 (1950), and the origin at alpha = 17h 42.4m, delta = -28 55 (1950). deg GLAT Galactic latitude deg SGLON Supergalactic longitude on RC2 sys. deg SGLAT Supergalactic latitude on RC2 sys. deg name Name Names (e.g., LMC, SMC) or NGC and IC designations. --- altname Alternate name UGC (Nilson 1973), ESO (Lauberts 1982), MCG (Vorontsov-Velyaminov et al. 1962-1974), UGCA (Nilson 1974), and CGCG (Zwicky et al. 1961-1968) designations, given in that order of preference. MCG designations not listed here are given in UGC and ESO. --- desig Other designation --- PGC PGC number PGC (Paturel et al. 1989a,b) designation. For cross identifications of various catalogues with the PGC, see Appendix 10, page 561. --- type Type Mean revised morphological type in the RC2 system, coded as in RC2 (Section 3.3.a, page 13). --- typesr Source of revised type "V" indicates a classification by de Vaucouleurs; "4" indicates a ring galaxy classified by Buta on 4-meter plates. --- T T (Hubble stage) Mean numerical index of stage along the Hubble sequence in RC2 system (coded as explained in Section 3.3.c, page 16). --- e_T Mean error of T --- lumcl Luminosity class(Section 3.3.d,p18) --- e_lumcl Mean error on luminosity class --- o_lumcl Num. of luminosity class estimates --- d25 Log D25 Mean decimal logarithm of the apparent major isophotal diameter measured at or reduced to surface brightness level muB = 25.0 B/mag2, as explained in Section 3.4.a, page 21. The unit of D is 0.1 arcmin to avoid negative entries. 0.1arcmin u_d25 indicates Log D25 very uncer. --- e_d25 Mean error on log D25 A "?" indicates a large, uncertain error. 0.1arcmin R25 Log R25 (isophotal diameter ratio) Mean decimal logarithm of the ratio of the major isophotal diameter, D25, to the minor isophotal diameter, d25, measured at or reduced to the surface brightness level muB = 25.0 B/mag2, and its mean error as explained in Section 3.4.b, page 26. --- u_R25 indicates Log R25 very uncertain --- e_R25 Mean error on log R25 A "?" indicates a large, uncertain error. --- Do Log Do Decimal logarithm of the isophotal major diameter corrected to "face-on" (i = 0), and corrected for galactic extinction to Ag = 0, but not for redshift, as explained in Section 3.4.d, page 29. 0.1arcmin Ae Log Ae (effective aperture) Decimal logarithm of the apparent diameter (in 0.1 arcmin) of the "effective aperture," the circle centered on the nucleus within which one-half of the total B-band flux is emitted, derived as explained in Section 3.4.c, page 28. 0.1arcmin e_Ae Mean error on log Ae 0.1arcmin PA Position angle of the major axis Position angle, measured in degrees from north through east (all <180), taken when available from UGC, ESO, and ESGC (and in a few cases from H I data) (Section 3.5.a, page 30). deg BT BT (total B magnitude) BT = total (asymptotic) magnitude in the B system derived by extrapolation from photoelectric aperture- magnitude data, BAT, and from surface photometry with photoelectric zero point, BSTas explained in Section 3.6.a, page 32. mag BT_code BT code "M" = BT is the weighted mean of BAT and BST, "S" = only surface photometry used "V" = BT is a V-band magnitude rather than a B-band magnitude "v" = the nucleus of the galaxy is variable. "*" indicates that deriving BAT would have required an extrapolation in excess of 0.75 mag. --- e_BT Mean error on BT mag Bmag mB (photographic magnitude) Photographic magnitude and its mean error from Ames (1930), Shapley and Ames (1932), CGCG, Buta and Corwin (1986), and/or Lauberts and Valentijn (1989) reduced to the BT system as explained in Section 3.6.b, page 37. mag e_Bmag Mean error on Bmag mag BoT BoT Total "face-on" magnitude corrected for galactic and internal extinction, and for redshift as explained in Section 3.6.d, page 44. mag m'25 m'25 The mean surface brightness in magnitudes per square arcmin (B-m/sm) within the muB = 25.0 B-m/ss elliptical isophote of major axis log D25 and axis ratio log R25, defined as in RC2 (Equation 21) by: m'25= BT + delta(m25) + 5 logD25- 2.5 logR25- 5.26, where delta(m25) = 2.5 log LT/L25 = B25 - BT and is the magnitude increment contributed by the outer regions of a galaxy fainter than muB = 25.0B-m/ss and, its mean error. For details, see Section 3.8.b, page 50. mag/arcmin2 e_m'25 Mean error m'25 mag/arcmin2 m'e m'e Mean B-band surface brightness in magnitudes per square arcmin (B-m/sm) within the effective aperture Ae, and its mean error, calculated by the relation m'e= BT + 0.75 + 5 logAe- 5.26. This m'e is statistically related to the effective mean surface brightness, mu'e (RC2, p. 31; Olson and de Vaucouleurs 1981), with which it coincides when log R = 0 (i = 0) (Section 3.8.a, page 49). mag/arcmin2 e_m'e Mean error m'e mag/arcmin2 mFIR mFIR Calculated from mFIR = -20.0 - 2.5 logFIR, where FIR is the far infrared continuum flux measured at 60 and 100 microns as listed in the IRAS Point Source Catalog (1987) <II/125>. For galaxies larger than 80 in RC2 and for the Virgo cluster area, resolved by the IRAS beam, integrated fluxes are taken from Rice et al.(1988) or Helou et al.(1988). See Section 3.6.c, page 43, for details. mag m21 m21 21-cm emission line magnitude defined by m21 = 21.6 - 2.5 log SH , where SH is the measured neutral hydrogen flux density in units of 10-24W/m2. For details, see Section 3.9.a, page 51. mag e_m21 Mean error on m21 mag B-VT (B-V)T (total (B-V)) Total (asymptotic) color index in the Johnson B-V and U-B system, respectively, derived by extrapolation from photoelectric color-aperture data, and/or from surface photometry with a photoelectric zero point as explained in Section 3.7.a, page 45. mag e_B-VT Mean error on (B-V)T mag B-Ve (B-V)e (mean B-V within Ae) Mean B-V and U-B color indices, respectively, within the effective aperture Ae, derived by interpolation from photoelectric color-aperture data as explained in Section 3.7.a, page 45. mag e_B-Ve Mean error on (B-V)e mag B-VoT (B-V)oT Total B-V and U-B color indices, respectively, corrected for galactic and internal extinction, and for redshift, as explained in Section 3.7.b, page 47. mag U-BT (U-B)T (total (U-B)) mag e_U-BT Mean error on (U-B)T mag U-Be (U-B)e mag e_U-Be Mean error on (U-B)e mag U-BoT (U-B)To mag HI HI (neutral hydrogen index) Corrected neutral hydrogen index, which is the difference mo21-BoT between the corrected (face-on) 21-cm emission line magnitude and the similarly corrected magnitude in the BT system. Details are given in Section 3.9.c, page 52. Since m21 and BT are listed separately in columns 6 and 9, record 1, there is no need to print the uncorrected index. mag Ai Ai (internal B extinction) Internal extinction in B-band magnitudes (for correction to face-on), calculated from log R and T as explained in Section 3.5.c, page 31. mag A21 A21 (HI self absorption) A21 = H I line self-absorption in magnitudes (for correction to face-on), calculated from log R and T greater or equal to 1 as explained in Section 3.5.d, page 32. mag Ag Ag (galactic extinction in B) Galactic extinction in B-band magnitudes, calculated following Burstein and Heiles (1978a,b, 1982, 1984) as explained in Section 3.5.b, page 30. mag W20 W20 Neutral hydrogen line full width (in km/s) measured at the 20% level (I20/Imax) and the 50% level (I50/Imax), respectively, as explained in Section 3.9.b, page 51. km/s e_W20 Mean error on W20 km/s W50 W50 km/s e_W50 Mean error of W50 km/s V21 V21 (heliocentric radial velocity) The mean heliocentric radial velocity derived from neutral hydrogen observations, as explained in Section 3.10.a, page 52. km/s e_V21 Mean error on V21 km/s cz Vopt= cz The mean heliocentric radial velocity, derived from optical observations, as explained in Section 3.10.b, page 53. km/s e_cz Mean error on Vopt km/s VGSR VGSR The weighted mean of the neutral hydrogen and optical velocities, corrected to the "Galactic standard of rest", as explained in Section 3.10.c, page 54. km/s V3K V3K The weighted mean velocity corrected to the reference frame defined by the 3K microwave background radiation, as explained in Section 3.10.d, page 55. km/s Nancy G. Roman SSDOO/ADC Francois Ochsenbein CDS 1995 Feb 16 We sincerely thank Dr. Harold Corwin for sending us the RC3 and the LaTeX version of the introduction. We also thank him for extensive advise during the production of the original document and for a careful reading of this final product. We thank Dr. Francois Ochsenbein for help in formatting this document. UNKNOWN UNKNOWN * 16-Feb-1995: Documentation done by Nancy G. Roman [SSDOO/ADC] * 28-Oct-1995: the values of RA (1950 and 2000) originally reported with a 0.1 min were converted to seconds at CDS (see notes above on RAs and RAs1950) UNKNOWN UNKNOWN NOTE: The references with many of the descriptions are to the page numbers in Volume 1 of the printed catalogue. Construction of the current version of the RC3: The RC3 was received electronically from Dr. Harold Corwin. It was transferred to a Dec-alpha work station for examination and then to a Cray computer for processing and archiving. Dr. Corwin also provided the introduction to the catalogue in LaTeX for the original version of the Third Reference Catalog. This introduction has been modified for the present document. Several changes were made in the catalogue. The printed version contained plus/minus signs. Since the eighth bit, which distinguishes special characters, tends to be dropped when the file is transferred electronically, these have all been removed; the meaning is obvious. The original version of the catalog contained four records for each galaxy. Those values in the same columns were often related. The catalog has been reformatted into a single record per galaxy and the order of the data has been changed to keep related information contiguous. Extra blank columns which resulted from the original structure have been removed, keeping a single blank between adjacent columns. VII_155.xml The Extended 12micron Galaxy Sample 7157 VII/157 The Extended 12um galaxy sample The Extended 12micron Galaxy Sample B Rush M Malkan L Spinoglio Astrophys. J. Suppl. Ser. 89 1 1993 1993ApJS...89....1R Galaxies, IR Galaxies, Seyfert Infrared sources Nonstellar objects Surveys The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.
The catalogue RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec F12 12 mu flux number=1 See file 12micron.doc or 12micron.tex Jy F25 25 mu flux number=1 See file 12micron.doc or 12micron.tex Jy F60 60 mu flux number=1 See file 12micron.doc or 12micron.tex Jy F100 100 mu flux number=1 See file 12micron.doc or 12micron.tex Jy Name Various name(s) of the source --- Type Object type number=2 Object type is 0=Normal 1=Seyfert-1 2=Seyfert-2 3=high-far-IR 4=LINER --- n_z Redshift type number=3 Redshift type is S=corrected for Galactic solar motion and for Galaxy's motion towards Virgo V=NOT corrected for motion towards Virgo --- r_z Redshift reference number=1 See file 12micron.doc or 12micron.tex --- z Redshift --- 12micron.doc Documentation 12micron.tex LaTeX documentation Francois Ochsenbein CDS 1994 Jul 20 VII_157.xml A Revised and Updated Catalog of Quasi-stellar Objects 7158 VII/158 Revised and Updated Catalog of Quasi-stellar Objects A Revised and Updated Catalog of Quasi-stellar Objects A Hewitt G Burbidge Astrophys. J. Suppl. Ser. 87 451 1993 1993ApJS...87..451H QSOs BL Lac objects This is a catalog of all known quasi-stellar objects (QSO's) with measured emission redshifts and BL Lac objects, complete to 1992 December 31. The catalog contains 7312 objects, nearly all QSOs including about 90 BL Lac objects. The catalog and references contain extensive information on names, positions, magnitudes, color, emission-line redshifts, absorption, variability, polarization, and X-ray, radio, and infrared data. A key in the form of subsidiary tables enables the reader to relate the name of a given object to its coordinate name which is used throughout the catalog.
The catalogue Extract of table1 (one line per quasar) CooDes Coordinate designation number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. --- RAh Right Ascension 1950 (hours) number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. h RAm Right Ascension 1950 (minutes) number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. min RAs Right Ascension 1950 (seconds) number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. s DE- Declination 1950 (sign) number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. --- DEd Declination 1950 (degrees) number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. deg DEm Declination 1950 (minutes) number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. arcmin DEs Declination 1950 (seconds) number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. arcsec BLLac "B" indicates a BL Lac object number=1 The fields in bytes 1-34 are repeated on each line for objects requiring more than one line; byte 35 is "+" for the second and continuation records. --- Sel Selection technique(s) number=2 Code for Selection technique(s): C = UV-excess O = Objective-prism and related techniques R = radio V = variability X = X-ray S = serendipity + + = continuation record as in Note (1) --- id Other name --- RA2h Right Ascension 2000 (hours) h RA2m Right Ascension 2000 (minutes) min RA2s Right Ascension 2000 (seconds) s DE2- Declination 2000 (sign) - DE2d Declination 2000 (degrees) deg DE2m Declination 2000 (minutes) arcmin DE2s Declination 2000 (seconds) arcsec V Apparent magnitude; often only mpg mag n_V * indicates a variability --- B-V B-V mag U-B U-B mag z(em) Emission redshift --- u_z(em) Uncertainty flag on z(em) --- n_z(em) Note on z(em) number=3 * = indicates that absorption redshifts have been reported + = absorption has been seen but no redshift systems have been measured --- Element Emission line on which the redshift is based (element name) --- Wl Wavelength of Emission element (Angstroem) 0.1nm z(abs) Absorption redshift --- r_id Reference for identification --- r_z(em) Reference for emission redshift (LBQS = Large Bright QSO Survey) --- ref_b Addition to r_z(em) --- ref_var Reference for variability --- ref_R Reference for Radio --- r_z(abs) Reference for absorption redshift --- Notes Notes number=4 Two lines of notes of the published table have been merged. The following abbreviations are used: B(J)mag: defined in Koo & Kron 1982 (A&A 105, 107) absr : 21cm absorption BAL : broad absorption line QSO BAL? : broad absorption lines questionable BALvar : broad absorption lines variable Bmag : COem : elp : emission-line profile emlvar : emission-lines variable euv : extreme ultra-violet spectra ext : report of optical jet or fuzz fc : finding chart FeIIem : many FeII lines hfe : high-frequency excess hpq : high polarization quasar imag : imaging ir : infrared ir/r : infrared/radio IRAS : object identified in IRAS catalogue irpol : infrared polarization irvar : infrared variable Jmag : defined in Koo & Kron 1982 (A&A 105, 107) m(or) : passband on direct plates used in IK Schmidt Survey mf : multifrequency observation mm : millimeter-wave observations mmvar : millimeter-wave variable neml : narrow emission lines noabs : OVV : optical violent variable phot : photometry pol : optical polarization poljet : polarized jet pos : position QSO? : r/ir : rjet : radio jet rmag : rmap : rnd : not detected as radio source rpol : radio polarization rvar : radio variable si : speckle interferometry sp : spectra spext : spectroscopy of the extension spvar : spectral variability sy1 : syi : ubv : colors ubvri : extended photometry uv : ultraviolet spectra uv/ir : spectrophotometry in the ultraviolet and near infrared uvabs : ultraviolet absorption uvem : ultraviolet emission uvnd : not detected in the ultraviolet uvvar : ultraviolet variable var? : varnd : variability not detected vlbi : very long baseline interferometry x : X-ray xnd : not detected as X-ray source xvar : X-ray variable Statistics on table1: 7315 objects average z (for objects with z > 0) = 1.56 290 objects with absorption seen but not measured, 415 with absorption measured discovered by also detected in total objective prism: 4145 0 4145 X-ray: 168 289 457 color/UV-excess: 1341 8 1349 radio: 1234 158 1392 --- References in numerical order References in alphabetical order Ref Reference number --- dot --- Text Reference text --- Nancy G. Roman (mod. J.A. Watko) SSDOO/ADC 1996 Dec 30 UNKNOWN UNKNOWN The files have been copied from the cass157.ucsd.edu (132.239.146.157) anonymous account on August 31, 1993. A standardization of the files and their description was performed at CDS to allow automatic conversions to FITS tables. Most of this document was prepared at the CDS. The description, ADC Keywords and Bibcode were added and portions of the format table were modified by the undersigned. We thank the CDS for forwarding the catalog and accompanying document. VII_158.xml Study of a field in the Coma Supercluster. I. Automated galaxies count 7159 VII/159 Catalogue of galaxies towards the Coma Supercluster Study of a field in the Coma Supercluster. I. Automated galaxies count E Slezak G Mars A Bijaoui C Balkowski P Fontanelli Astron. Astrophys. Suppl. Ser. 74 83 1988 1988A&AS...74...83S Clusters, galaxy galaxies: clusters: individual (Coma) image processing in astronomy galaxy count Schmidt plate analysis The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.
*Galaxies towards the Coma Supercluster NmB18 Object number for the galaxies brighter than the 18th magnitude (otherwise 0). --- N Object number --- RAh right ascension (hours) (J2000) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination (degrees) (J2000) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec Bmag B magnitude mag MType morphological type --- Note SIMBAD or velocity note number=1 the symbol is: '*' = object with identification in SIMBAD (Strasbourg Data Center). 'v' = object with a known radial velocity. --- Koichi Nakajima CDS 1993 Sep 27 UNKNOWN UNKNOWN The catalogue was provided by courtesy of E. Slezak to H. Andernach; it was numbered A100 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 01-Oct-1993: First archived. 12-Jan-1994: "Intro" file has been slightly rewritten. (The date of the latest archive, see the date of each file.) 08-Aug-1997: this documentation has been standardized at CDS (Francois Ochsenbein) VII_159.xml Nearby Galaxies. 7161 VII/161 Nearby Galaxies Nearby Galaxies. K -H Schmidt A Priebe Th Boller Astron. Nachr. 314 371 1993 1993AN....314..371S VII/98 : Catalogue of 2810 nearby galaxies (Kraan-Korteweg, 1986) VII/145 : Nearby Galaxies Catalogue (NBG) (Tully 1988) Young, J.S., Shuding Xie, Kenney, J.D.P., Rice, W.L. 1989, =1989ApJS...70..699Y Karachentsev, I. 1993, Special Astrophys. Obs. A.S. U.S.S.R., Preprint 100 Kraan-Korteweg, R.C., Tammann, G.A.: 1979, Astron. Nachr., 300, 181. Schmidt, K.-H., Boller, T.: 1992, Astron. Nachr., 313, 189. =1992AN....313..189S Galaxies, nearby The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt & Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).
The Catalogue SPB Running number in order of RA1950 --- Name Name (or comma-separated list of names) --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin HVel Heliocentric velocity km/s vLG1 Velocity adjusted for solar motion (method 1) km/s Group Group membership --- u_Group Uncertainty flag [:] on Group --- i Inclination (face-on, in degrees) deg BT Observed total photoelectric blue mag. mag u_BT Uncertainty flag on BT number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- BT(0,i) Blue corrected magnitude (adjusted for galactic and internal extinction) mag u_BT(0,i) Uncertainty flag on BT(0,i) number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- (B-V)T Observed total colour index mag (U-B)T Observed total colour index mag logD25 Logarithm of the angular diameter D25 0.1arcmin u_logD25 Uncertainty flag on logD25 number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- e_logD25 Error for logD25 0.1arcmin S Integrated H I flux Jy.km/s u_S Uncertainty flag on S number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- Vmax Maximal rotational velocity km/s u_Vmax Uncertainty flag on Vmax number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- Dv50 H I line width (50 per cent peak width) km/s u_Dv50 Uncertainty flag on Dv50 number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- o_Dv50 Number of measurements for Dv50 --- IRAS Name of the main infrared source from the IRAS catalogue (1988) (several for more than one possible identification) --- sample cf. detailed explanation in Schmidt and Boller (1992) --- Name1 Alternate name(s) --- GLON Galactic longitude (in degrees) deg GLAT Galactic latitude (in degrees) deg e_HVel Adopted error for HVel km/s vLG2 Velocity adjusted for solar motion (method 2) km/s Theta Angular distance from the center of the Virgo cluster deg Ag Galactic extinction in mag mag u_Ag Uncertainty flag on Ag number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- Bmag Blue photographic magnitude mag u_Bmag Uncertainty flag on mB number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- MB Absolute magnitude mag u_MB Uncertainty flag on MB number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- (B-V)T0 Total colour index (corrected for galactic and external reddening) mag u_(B-V)T0 Uncertainty flag on (B-V)T0 number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- (U-B)T0 Total colour index (corrected for galactic and external reddening) mag u_(U-B)T0 Uncertainty flag on (U-B)T0 number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- logR25 Logarithm of the axis ratio R25 --- u_logR25 Uncertainty flag on logR25 number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- e_logR25 Mean error for logR25 --- e_S Mean error for S Jy.km/s u_e_S Uncertainty flag on e_S number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- maxVmax Maximum of the maximal observed rotational velocity km/s u_maxVmax Uncertainty flag on maxVmax number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- Dv20 H I line width (20 per cent peak width) km/s u_Dv20 Uncertainty flag on Dv20 number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- o_Dv20 Number of measurements for Dv20 --- logFIR Logarithm of the far-infrared-flux (erg/cm2/s) mW/m2 u_logFIR Uncertainty flag on logFIR number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- x2(ind) Individual relative distance --- Name2 Alternate name(s) --- SLON Supergalactic longitude deg SLAT Supergalactic latitude deg vLG3 Velocity adjusted for solar motion (method 3) km/s x2 Distance of the galaxy in units of the distance of the Virgo cluster --- u_x2 Uncertainty flag for x2 number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- Ai Internal extinction mag u_Ai Uncertainty flag on Ai number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- n_type 'p' for peculiar --- type Morphological type (numerical encoded) --- u_type Uncertainty flag on type number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- e_type Uncertainty for the type of the galaxy (numerical encoded) --- u_e_type Uncertainty flag on e_type number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- logD0 Logarithm of the corrected diameter 0.1arcmin u_logD0 Uncertainty flag on logD0 number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- logMHI Logarithm of HI mass solMass u_logMHI Uncertainty flag on logMHI number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- o_Vmax Number of measurements for Vmax --- DV0.i Corrected H I line width km/s u_DV0.i Uncertainty flag for DV0,i number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- logMdust Logarithm of the dust mass solMass u_logMdust Uncertainty flag for logMdust number=1 The uncertainty flags have the following meaning: < lower or equal (upper value) : uncertain # very uncertain --- Francois Ochsenbein CDS 1993, rev. 10-Jun-1996 Oct 13 We thank Drs Karl-Heinz Schmidt <khschmidt@aip.de> and Andreas Priebe <apriebe@aip.de> for reviewing the short documentation in October 1993. UNKNOWN UNKNOWN The catalogue was copied in October 1993 from anonymous ftp at node ftp://ftp.aip.de/pub/catalogues/nearby_galaxies. A few realignments have been performed; there were two SPB#015, and the first one was transformed into SPB#013. VII_161.xml Flat Galaxy Catalogue 7162 VII/162 Flat Galaxy Catalogue Flat Galaxy Catalogue I D Karachentsev V E Karachentseva S L Parnovsky Astron. Nachr. 314 97 1993 1993AN....314...97K Galaxy catalogs Nonstellar objects galaxies: spiral catalogs A systematic search for disklike edge-on galaxies with a diameter larger than a=40 arcsec and major-to-minor axis ratio a/b>7 has been carried out by means of Palomar Observatory Sky Survey and ESO/SERC survey. As a result, we present new catalog of a flat galaxies (FGC) containing 4455 objects and covering about 56% of the whole sky for the first time. The catalog is assigned to study large-scale cosmic streamings and another problems of observational cosmology. Due to a better quality of the photographic emulsions used for the southern sky survey, the galaxies measured on ESO/SERC films extend to a surface magnitude slightly fainter than the same galaxies measured on POSS prints. So we present the catalog data separately for northern sky (DEC from -17.5 to +90 degrees) - FLAT GALAXY CATALOG , FGC, N = 2573 and for southern sky (DEC from -90 to -17.5 degrees) - SOUTHERN EXTENSION OF FLAT GALAXY CATALOG, FGCE, N = 1882. There are about 200 galaxies in a common region which were found and measured independently on POSS prints and ESO/SERC films. They were included in FGC, not in FGCE. The mean ratio <a(ESO)/a(POSS)> for them is equal to 1.26+/-0.4. This value is near to the result obtained by Lauberts (1982). Making some statistics it is easy to exclude FGCE galaxies with a <50arcsec to have the same depth of the sample. The Appendix to Flat Galaxy Catalog - Addendum - contains the data of 291 galaxies. They were selected in preliminary survey but rejected after more precise diameter measurements because of violation the a/b >= 7 criterion. In every case, these galaxies can be used in different observational programs.
FGC and FGCE catalogues Appendix to FGC FGC Galaxy FGC or FGCE (E in col.1) number or addendum (A in col.5); --- PGC Identification number with Catalogue of Principal Galaxies (PGC, Paturel et al, 1989); --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg aO Major diameter measured on blue prints/films arcmin bO Minor diameter measured on blue prints/films arcmin aE Major diameter measured on red prints/films arcmin bE Minor diameter measured on red prints/films arcmin PA Positional angle of galaxy major axis measured from North towards East; deg T Morphological type of spiral according to Hubble classification; --- As Index of apparent asymmetry Index of apparent asymmetry: 0 - feebly marked 2 - pronounced The features of asymmetry may be: - different length of spiral arms, - symmetry in the luminosity distribution, - resence of bright knots, - distortion of galaxy shape and so on. --- SB Index of mean surface brightness ( I - high, IV - very low). --- N Number of significant neighbors N are the number of significant neighbors having an angular diameter in the range from 2a to a/2 and located in the circle of R=10a , where a is major axis of galaxy considered. --- Notes A star indicates the presence of a note. --- Alternate names of FGC and FGCE galaxies FGC Galaxy FGC or FGCE --- PGC PGC name --- c1 flag: '?' (PGC questionable), '(' (concerns the next name) or '=' (two different PGC numbers) --- Names Alternate names, normally up to 4 names (format 4A16) there are however exceptions. --- Notes to FGC and FGCE galaxies FGC Galaxy FGC or FGCE --- Text Text of the note --- N. Paul Kuin ADC 1997 May 13 Authors are very grateful to O.A.Dobrodij, G.G.Korotkova,. and M.E.Sharina taken part in coordinate measurements of flat galaxies. We thank Dr. Yu.N.Kudrya for great help in the preparation of the Catalog and Dr. G.Paturel who kindly presented the diskettes with Principal Galaxy Catalog version. The Intro documentation that froms the basis for this document was authored by Francois Ochsenbein [CDS] 14-Oct-1993. Author's Addresses: I.D.Karachentsev, Zelenchukskaya, Russia Special Astrophysical Observatory V.E.Karachentseva, S.L.Parnovsky, Kiev, Ukraine Astronomical observatory of Kiev University VII_162.xml A Catalogue of Measured Redshifts of Abell Clusters of Galaxies 7165 VII/165 Cat of Measured Redshifts of Abell Clusters of Gal A Catalogue of Measured Redshifts of Abell Clusters of Galaxies H Andernach ASP Conf. Ser. 15 279 1991 VII/110 : The "ACO-catalogue" (Abell+ 1989) Clusters, galaxy Redshifts The 'ACO' catalog (Abell, Corwin and Olowin 1989) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.
Measured redshifts of Abell clus. of galaxies Prefix prefix for the cluster name 'A' for rich clusters, 'S' for ACO extension of poor or distant clusters. --- IDnum numbering part of the cluster name --- Suffix suffix for the cluster name --- RAh right ascension (hours) (B1950) Right ascension and declination of the cluster center, as of ACO h mRAm right ascension (0.1minutes) 0.1min DE- declination sign --- DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin RICH Abell richness class --- DIST Abell distance class --- BM Bautz-Morgan class --- q_BM quality code of BM, as of ACO --- m10 magnitude of the 10th brightest cluster member 0.1mag q_Z quality code of redshift See "expl.txt" file. --- Z cluster redshift 10-4 r_Z reference code of redshift --- Arad Abell radius (=3 Mpc/Ho/50),using qo=0.10 0.1arcmin log(Zm/Ze) The ratio between measured and estimated z --- expl.txt Explanation file K. Nakajima, H. Andernach CDS ; C.-H. Lyu Hughes STX/NASA 1996 Oct 31 The original expl(anation).txt file by Andernach (1991) was used to create this ReadMe file. VII_165.xml Catalogue of Double Galaxies in the region of Southern Galactic Cap 7168 VII/168 Double Galaxies in SGP region Catalogue of Double Galaxies in the region of Southern Galactic Cap Z Zou J Chen X Tang Y Bian Bull. Inf. CDS 37 173 1989 1989BICDS..37..173Z Catalogue of Double Galaxies in the region of Southern Galactic Cap Z Zou J Chen X Tang Y Bian Publ. of the Beijing Astron. Observatory 12 8 1989 1989PBeiO..12....8Z Galaxy catalogs 630 double systems of galaxies brighter than about 17mag(B) were found by examining 100 glass copies of ESO(B) survey plates, covering the Southern Galactic Cap (GLAT<-50deg, DE<-27deg). The selection criteria are similar to those defined by Zonn (1962). The measuring, reduction and error analysis parameters have been described by Zou et al. (1984).
The Catalogue of double galaxies Pair Name of the galaxy pair number=1 the pair name is made of plate number (4 bytes), decimal point, and an ordinal number by increasing RA --- RAh Right Ascension 1950 of W component (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) number=2 mean error on position of components is about 2arcsec s DE- Declination 1950 of W component (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) number=2 mean error on position of components is about 2arcsec arcsec MType Morphological (Hubble) type of W component --- Bmag B magnitude of W component number=3 mean error about 2mag mag Rmaj Major radius of W component number=4 relative error about 0.1 (10%) arcsec Rmin Minor radius of W component number=4 relative error about 0.1 (10%) arcsec paRmaj Position angle of W component number=5 position angle North to East, mean error about 5deg deg RAh2 Right Ascension 1950 of W component (hours) h RAm2 Right Ascension 1950 (minutes) min RAs2 Right Ascension 1950 (seconds) number=2 mean error on position of components is about 2arcsec s DE-2 Declination 1950 (sign) of E component --- DEd2 Declination 1950 (degrees) deg DEm2 Declination 1950 (minutes) arcmin DEs2 Declination 1950 (seconds) number=2 mean error on position of components is about 2arcsec arcsec MType2 Morphological type of E component --- Bmag2 B magnitude of E component number=3 mean error about 2mag mag Rmaj2 Major radius of E component number=4 relative error about 0.1 (10%) arcsec Rmin2 Minor radius of E component number=4 relative error about 0.1 (10%) arcsec paRmaj2 Position angle of E component number=5 position angle North to East, mean error about 5deg deg Sep Angular separation of the two galaxies, mean error about 1arcsec. arcsec paSep Position angle of separation vector, North to East, mean error 2deg. deg K. Nakajima CDS Sep-1994 F. Ochsenbein, H. Andernach CDS 1996 Jun 13 UNKNOWN UNKNOWN Thanks are due to Heinz Andernach <hja@vilspa.esa.es> for asking the catalogue to the author in Nov. 1990; he took care of checking and correcting the catalogue, in interaction with Zou Zhenlong <zouzl@bepc2.ihep.ac.cn>. VII_168.xml The identifications of IRAS point sources - I. A 304 deg^2 field centred on the South Galactic Pole 7169 VII/169 Optical Identifications of IRAS Point Sources The identifications of IRAS point sources - I. A 304 deg^2 field centred on the South Galactic Pole R D Wolstencroft A Savage R G Clowes H T MacGillivray S K Leggett M Kalafi Mon. Not. R. Astron. Soc. 223 279 1986 1986MNRAS.223..279W The identifications of IRAS point sources - I. A 304 deg^2 field centred on the South Galactic Pole S K Leggett R G Clowes M Kalafi H T MacGillivray P J Puxley A Savage R D Wolstencroft Mon. Not. R. Astron. Soc. 227 563 1987 1987MNRAS.227..563L The identifications of IRAS point sources - I. A 304 deg^2 field centred on the South Galactic Pole G Wang R G Clowes S K Leggett H T MacGillivray A Savage MNRAS 248 112 1991 1991MNRAS.248..112W Clusters, galaxy Galactic pole, south Optical identifications are given of IRAS point sources: 312 sources in a 304 square deg area centred on the South Galactic Pole, of which 148 are identified with stars, 154 with galaxies and 10 are unidentified down to 21st magnitude; 206 point sources in a 113 square deg area centred on the Virgo cluster, of which 54 are identified with stars, 113 with optically bright (B_J<16) galaxies, 32 with faint galaxies, and 7 are apparently empty fields; (66, 114, 61) sources in the regions of (Fornax, Hydra I, Coma) cluster of galaxies, of which (35, 48, 18) are identified with stars, (43, 58, 41) with galaxies.
optical identifications in the South Galactic Pole region IRAS IRAS name by IAU format --- RAh IRAS right ascension (hours) (B1950) h RAm IRAS right ascension (minutes) min RAs IRAS right ascension (seconds) s DE- declination sign --- DEd IRAS declination (degrees) (B1950) deg DEm IRAS declination (minutes) arcmin DEs IRAS declination (seconds) arcsec SMAJ IRAS position uncertainty semi-major axis number=1 See IRAS Point Source Catalog. arcsec SMIN semi-minor axis of above number=1 See IRAS Point Source Catalog. arcsec THETA orientation of SMAJ, east of equatorial north number=1 See IRAS Point Source Catalog. deg F12 IRAS flux density at 12micron number=1 See IRAS Point Source Catalog. Jy l_F12 upper limit flag of F12 --- F25 IRAS flux density at 25micron number=1 See IRAS Point Source Catalog. Jy l_F25 upper limit flag of F25 --- F60 IRAS flux density at 60micron number=1 See IRAS Point Source Catalog. Jy l_F60 upper limit flag of F60 --- F100 IRAS flux density at 100micron number=1 See IRAS Point Source Catalog. Jy l_F100 upper limit flag of F100 --- ANAME association name in IRAS (1) number=2 See IRAS Explanatory Supplement V.H.9. --- OFF_RA offset (optical - IRAS) for east of RA arcsec OFF_DE offset (optical - IRAS) for north of DE arcsec TYPE morphological type for galaxy, or spectral class for star number=3 Spectral class and magnitude of the star is taken from SAO or Bright Star Catalogues. --- BJmag for galaxy, B_J magnitude integrated above the 25 mag of COSMOS isophoto, for star, V magnitude number=3 Spectral class and magnitude of the star is taken from SAO or Bright Star Catalogues. mag f1_BJcos flag for COBJ (not explained in paper) --- BJcos B_J magnitude measured by COSMOS mag f2_BJcos flag for COBJ (not explained in paper) --- NOTES additional notes number=4 For abbreviations, see paper p293. 'R' denotes extra remarks on individual sources at the end of the Table in the paper. --- optical identifications in the Virgo cluster region IRAS IRAS name by IAU format --- b1_RADE open bracket for IRAS position number=1 For empty fields the IRAS position is given in brackets. --- RAh COSMOS right ascension (h) (B1950) number=1 For empty fields the IRAS position is given in brackets. h RAm COSMOS right ascension (minutes) number=1 For empty fields the IRAS position is given in brackets. min RAs1 COSMOS right ascension (0.1s) number=1 For empty fields the IRAS position is given in brackets. 0.1s DE- declination sign number=1 For empty fields the IRAS position is given in brackets. --- DEd COSMOS declination (degrees) (B1950) number=1 For empty fields the IRAS position is given in brackets. deg DEm COSMOS declination (minutes) number=1 For empty fields the IRAS position is given in brackets. arcmin DEs COSMOS declination (seconds) number=1 For empty fields the IRAS position is given in brackets. arcsec b2_RADE close bracket for IRAS position number=1 For empty fields the IRAS position is given in brackets. --- OFF_RA offset (optical - IRAS) for RA arcsec OFF_DE offset (optical - IRAS) for DE arcsec NAME name of optical source --- TYPE morphological classification: galaxies by eye following de Vaucouleurs (1959); stars from number=2 Spectral class and magnitude of the star is taken from SAO or The Bright Star Catalogues. For the few uncatalogued stars, B magnitude is estimated from the diffraction spike length on the plate. --- TCODE type code, see p569 of the paper --- BJmag for galaxy, B_J magnitude either from catalogues or estimated off the plate above the 25 mag of COSMOS isophoto; for star, V magnitude number=2 Spectral class and magnitude of the star is taken from SAO or The Bright Star Catalogues. For the few uncatalogued stars, B magnitude is estimated from the diffraction spike length on the plate. mag BJcos B_J magnitude measured by COSMOS mag F12 IRAS flux density at 12micron number=3 Not color corrected. Jy l_F12 quality flag of F12 number=4 'L' denotes values that are upper limits only, ':' denotes moderate quality fluxes. --- F25 IRAS flux density at 25micron number=3 Not color corrected. Jy l_F25 quality flag of F25 number=4 'L' denotes values that are upper limits only, ':' denotes moderate quality fluxes. --- F60 IRAS flux density at 60micron number=3 Not color corrected. Jy l_F60 quality flag of F60 number=4 'L' denotes values that are upper limits only, ':' denotes moderate quality fluxes. --- F100 IRAS flux density at 100micron number=3 Not color corrected. Jy l_F100 quality flag of F100 number=4 'L' denotes values that are upper limits only, ':' denotes moderate quality fluxes. --- logIROP log. of ratio of far-IR luminosity to optical luminosity number=5 Ratios are given for those galaxies with better than upper limit detections at both 60 and 100microns, and that have COSMOS B-magnitudes. --- logFIR log. of far-IR luminosity in units of solar lum. for those galaxies with measured redshifts and better than upper limit detections at both 60 and 100microns --- NOTES notes of flags given in IRAS Point Source Catalogue, and for further remarks number=6 For abbreviations, see paper p569. 'R' denotes extra remarks on individual sources at the end of the Table in the paper, p569. --- optical identifications in the Fornax, Hydra I, Coma cluster regions IRAS IRAS name by IAU format (in Coma part, "x1247+257" is written once) --- RAh COSMOS right ascension (h) (B1950) number=1 COSMOS positions are measured from UKST plates (see paper p113L). For some objects on the edges of plates, catalogue positions are given. For empty fields the IRAS Point Source Cat. position is given. h RAm COSMOS right ascension (minutes) number=1 COSMOS positions are measured from UKST plates (see paper p113L). For some objects on the edges of plates, catalogue positions are given. For empty fields the IRAS Point Source Cat. position is given. min RAs1 COSMOS right ascension (0.1s) number=1 COSMOS positions are measured from UKST plates (see paper p113L). For some objects on the edges of plates, catalogue positions are given. For empty fields the IRAS Point Source Cat. position is given. 0.1s DE- declination sign number=1 COSMOS positions are measured from UKST plates (see paper p113L). For some objects on the edges of plates, catalogue positions are given. For empty fields the IRAS Point Source Cat. position is given. --- DEd COSMOS declination (degrees) (B1950) number=1 COSMOS positions are measured from UKST plates (see paper p113L). For some objects on the edges of plates, catalogue positions are given. For empty fields the IRAS Point Source Cat. position is given. deg DEm COSMOS declination (minutes) number=1 COSMOS positions are measured from UKST plates (see paper p113L). For some objects on the edges of plates, catalogue positions are given. For empty fields the IRAS Point Source Cat. position is given. arcmin DEs COSMOS declination (seconds) number=1 COSMOS positions are measured from UKST plates (see paper p113L). For some objects on the edges of plates, catalogue positions are given. For empty fields the IRAS Point Source Cat. position is given. arcsec OFF_RA offset (optical - IRAS) for RA arcsec OFF_DE offset (optical - IRAS) for DE arcsec F12 IRAS flux density at 12micron Jy l_F12 quality flag of F12 number=2 'L' denotes values that are upper limits only, ':' denotes moderate quality fluxes. --- F25 IRAS flux density at 25micron Jy l_F25 quality flag of F25 number=2 'L' denotes values that are upper limits only, ':' denotes moderate quality fluxes. --- F60 IRAS flux density at 60micron Jy l_F60 quality flag of F60 number=2 'L' denotes values that are upper limits only, ':' denotes moderate quality fluxes. --- F100 IRAS flux density at 100micron Jy l_F100 quality flag of F100 number=2 'L' denotes values that are upper limits only, ':' denotes moderate quality fluxes. --- TYPE for galaxy, morphological classification followed de Vaucouleurs (1959); for star, spectral classification --- TCODE type code, see p113R of the paper --- BJmag for galaxy, COSMOS B_J magnitude; for star, B magnitude (see paper p113R) mag q_BJmag 'e' denotes that B magnitude for star is estimated from the catalogued V and the B-V (see paper p113R) --- Bmag_cat catalogue magnitude: for galaxy, the catalogued B, or B_J estimated from plates by comparing the images with known mag.; for star, catalogued (Bright Star or SAO) V magnitude mag NAME name in optical catalogue, such as NGC, ESO, SAO, BS, etc. --- NOTES notes of flags given in IRAS Point Source Catalogue, and for further remarks number=3 For abbreviations, see paper p113R. 'R' denotes extra remarks on individual sources at the end of the Table in the paper, p117. --- N. Paul Kuin ADC 1997 May 12 UNKNOWN UNKNOWN The catalogue was provided by courtesy of S.K. Leggett to H. Andernach; it was numbered A120 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 13-Feb-1994: First archived. Intro file by Koichi Nakajima [CDS] 27-Sep-1993 The file "sgpi.dat" has been rearranged with shifting columns, in order to place the decimal points in the same column. Updated ReadMe document and filenames 12-May-1997 by Paul Kuin [ADC] VII_169.xml Catalogue of Southern Peculiar Galaxies and Associations. Volume I. Positions and descriptions. 7170 VII/170 Catalogue of Southern Peculiar Galaxies and Associations Catalogue of Southern Peculiar Galaxies and Associations. Volume I. Positions and descriptions. H C Arp B F Madore Cambridge University Press ??? ??? 1987 1987AMCat.C......1A VII/74 : Atlas of (Northern) Peculiar Galaxies (Arp =1966ApJS...14....1A) Galaxy catalogs Clusters, galaxy This "Catalogue of Southern Peculiar Galaxies and Associations" is a complete and detailed catalogue of all the most interesting galaxies and most striking apparent associations of galaxies in the Southern sky. The printed catalogue is made of two volumes: Volume I which lists the Peculiar Galaxies, and Volume II which contains photographs of galaxies which are representative of the various Categories used in the Classification scheme presented in Volume I.
Catalogue of Southern peculiar galaxies and associations FCflag * indicates that the object is illustrated in Volume II --- AM AM identification number=1 Note that the AM designation is based on the 1950 position with "format" HHMM+DDM, where the last 'M' digit represents truncated tens of arc minutes (the last digit is always between 0 and 5) --- n_AM More detailed AM identification number=2 For objects that are part of a pair, a triple or a larger association of objects which are also listed and described in the Catalogue as separate entries, this number represents the abbreviated right ascension and declination of the member immediately preceding the current object in order of right ascension (only the last number of right ascension and the four numbers of declination are given) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin GLON Galactic longitude deg GLAT Galactic latitude deg SGL Supergalactic longitude 0.1deg SGB Supergalacitc latitude 0.1deg n_Diam Note on Diam number=3 S or D, indicating that the following number is a measure of either the separation (S) of major components, or a characteristic diameter (D) of the system as a whole, respectively. --- Diam Diameter or Separation number=3 S or D, indicating that the following number is a measure of either the separation (S) of major components, or a characteristic diameter (D) of the system as a whole, respectively. 0.1arcmin CD1 Category number=4 the following Description Codes are used: 1 Galaxies with interacting companion(s) 2 Interacting doubles (galaxies of comparable size) 3 Interacting triples 4 Interacting quartets 5 Interacting quintets 6 Ring galaxies (or morphologically similar objects) 7 Galaxies with (linear) jets 8 Galaxies with apparent companion(s) 9 M51-types (companion at end of spiral arm) 10 Galaxies with peculiar spiral arms 11 Three-armed spirals and multiple-armed spirals 12 Peculiar disks (major asymmetry or deformation) 13 Compact (very high-surface-brightness) galaxies 14 Galaxies with prominent or unusual dust absorption 15 Galaxies with tails, loops of material or debris 16 Irregular or disturbed, (apparently isolated) galaxies 17 Chains (four or more galaxies aligned) 18 Groups (four or more galaxies not aligned) 19 Clusters (only very conspicuous, rich systems) 20 Dwarf galaxies (low surface brightness) 21 Stellar objects with associated nebulosity 22 Miscellaneous (rare or distinctive objects) 23 Close pairs (not visibly interacting) 24 Clode triples (not visibly interacting) 25 Planetary nebulae --- CD2 Category number=4 the following Description Codes are used: 1 Galaxies with interacting companion(s) 2 Interacting doubles (galaxies of comparable size) 3 Interacting triples 4 Interacting quartets 5 Interacting quintets 6 Ring galaxies (or morphologically similar objects) 7 Galaxies with (linear) jets 8 Galaxies with apparent companion(s) 9 M51-types (companion at end of spiral arm) 10 Galaxies with peculiar spiral arms 11 Three-armed spirals and multiple-armed spirals 12 Peculiar disks (major asymmetry or deformation) 13 Compact (very high-surface-brightness) galaxies 14 Galaxies with prominent or unusual dust absorption 15 Galaxies with tails, loops of material or debris 16 Irregular or disturbed, (apparently isolated) galaxies 17 Chains (four or more galaxies aligned) 18 Groups (four or more galaxies not aligned) 19 Clusters (only very conspicuous, rich systems) 20 Dwarf galaxies (low surface brightness) 21 Stellar objects with associated nebulosity 22 Miscellaneous (rare or distinctive objects) 23 Close pairs (not visibly interacting) 24 Clode triples (not visibly interacting) 25 Planetary nebulae --- CD3 Category number=4 the following Description Codes are used: 1 Galaxies with interacting companion(s) 2 Interacting doubles (galaxies of comparable size) 3 Interacting triples 4 Interacting quartets 5 Interacting quintets 6 Ring galaxies (or morphologically similar objects) 7 Galaxies with (linear) jets 8 Galaxies with apparent companion(s) 9 M51-types (companion at end of spiral arm) 10 Galaxies with peculiar spiral arms 11 Three-armed spirals and multiple-armed spirals 12 Peculiar disks (major asymmetry or deformation) 13 Compact (very high-surface-brightness) galaxies 14 Galaxies with prominent or unusual dust absorption 15 Galaxies with tails, loops of material or debris 16 Irregular or disturbed, (apparently isolated) galaxies 17 Chains (four or more galaxies aligned) 18 Groups (four or more galaxies not aligned) 19 Clusters (only very conspicuous, rich systems) 20 Dwarf galaxies (low surface brightness) 21 Stellar objects with associated nebulosity 22 Miscellaneous (rare or distinctive objects) 23 Close pairs (not visibly interacting) 24 Clode triples (not visibly interacting) 25 Planetary nebulae --- CD4 Category number=4 the following Description Codes are used: 1 Galaxies with interacting companion(s) 2 Interacting doubles (galaxies of comparable size) 3 Interacting triples 4 Interacting quartets 5 Interacting quintets 6 Ring galaxies (or morphologically similar objects) 7 Galaxies with (linear) jets 8 Galaxies with apparent companion(s) 9 M51-types (companion at end of spiral arm) 10 Galaxies with peculiar spiral arms 11 Three-armed spirals and multiple-armed spirals 12 Peculiar disks (major asymmetry or deformation) 13 Compact (very high-surface-brightness) galaxies 14 Galaxies with prominent or unusual dust absorption 15 Galaxies with tails, loops of material or debris 16 Irregular or disturbed, (apparently isolated) galaxies 17 Chains (four or more galaxies aligned) 18 Groups (four or more galaxies not aligned) 19 Clusters (only very conspicuous, rich systems) 20 Dwarf galaxies (low surface brightness) 21 Stellar objects with associated nebulosity 22 Miscellaneous (rare or distinctive objects) 23 Close pairs (not visibly interacting) 24 Clode triples (not visibly interacting) 25 Planetary nebulae --- CD5 Category number=4 the following Description Codes are used: 1 Galaxies with interacting companion(s) 2 Interacting doubles (galaxies of comparable size) 3 Interacting triples 4 Interacting quartets 5 Interacting quintets 6 Ring galaxies (or morphologically similar objects) 7 Galaxies with (linear) jets 8 Galaxies with apparent companion(s) 9 M51-types (companion at end of spiral arm) 10 Galaxies with peculiar spiral arms 11 Three-armed spirals and multiple-armed spirals 12 Peculiar disks (major asymmetry or deformation) 13 Compact (very high-surface-brightness) galaxies 14 Galaxies with prominent or unusual dust absorption 15 Galaxies with tails, loops of material or debris 16 Irregular or disturbed, (apparently isolated) galaxies 17 Chains (four or more galaxies aligned) 18 Groups (four or more galaxies not aligned) 19 Clusters (only very conspicuous, rich systems) 20 Dwarf galaxies (low surface brightness) 21 Stellar objects with associated nebulosity 22 Miscellaneous (rare or distinctive objects) 23 Close pairs (not visibly interacting) 24 Clode triples (not visibly interacting) 25 Planetary nebulae --- ESO/SERC ESO/SERC field number --- SERC-J SERC J plate number --- Xpos X position number=5 The Cartesian coordinates of the object are measured from the lower left-hand (south-east) corner of the original SERC plate. mm Ypos Y position number=5 The Cartesian coordinates of the object are measured from the lower left-hand (south-east) corner of the original SERC plate. mm Desc Description number=6 the following abbreviations are used: ABS'N. absorption APP. apparent ASSOC. association ASYMM. asymmetric BR. bright CIRC. circular COMP'N. companion COMP'NS. companions CONDENS. condensation CONN. connected/ing/ion DBL. double DIAM. diametric E elliptical ELONG. elongated ENVEL. envelope FILAM. filament FNT. faint G.D. grand design GAL./GALS. galaxy/galaxies GRP. group HI.S.BR. high surface brightness incl. including I/A interacting IRR. irregular LO.S.BR. low surface brightness MA.AX. major axis MATR'L material MDM.S.BR. medium surface brightness MI.AX. minor axis MULTI. multiple PEC. peculiar S.BR. surface brightness SP. spiral V. very w. with + and or plus --- Patricia Bauer CDS 1995, rev. Heinz Andernach [CDS] 11-Jun-1996 Jan 18 UNKNOWN UNKNOWN The machine file of the Arp & Madore Atlas of Peculiar Galaxies (1987) was kindly provided by B. Madore to H. Andernach in April 1991. A few formatting errors were detected by H. Andernach, corrected and commented to B.Madore that time. H. Andernach provided a copy to CDS in February 1993. Further formatting errors were detected and corrected at CDS. Two more errors (diameter of AM 0640-505 and Category of AM 1934-563) were detected by H. Andernach in June 1996 and corrected. VII_170.xml The First Byurakan Survey. A catalogue of galaxies with UV-continuum 7172 VII/172 First Byurakan Survey The First Byurakan Survey. A catalogue of galaxies with UV-continuum B E Markarian V A Lipovetsky J A Stepanian L K Erastova A I Shapovalova Comm. SAO USSR 62 ??? ??? 1989 1989SoSAO..62....5M Galaxies, Markarian Galaxies, UV-excess A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (<16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.
The FBS Catalogue of Markarian galaxies Mrk Markarian designation number --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec z0 Redshift corrected for Galaxy rotation (the rotation constant is Q=300km/s) --- Mag Apparent magnitude from the CGCG mag n_Mag An '*' indicates that there were no value in CGCG and that the magnitude given is the original estimates of the authors --- Mabs Absolute magnitude mag Sp Spectral type --- MajDiam Major axis diameter arcsec n_MajDiam Multiplicative symbol for angular size --- MinDiam Minor axis diameter arcsec r_z0 Redshift reference (See "refs.dat" file) --- n_Mrk A '*' indicates the double object having the same number in the original list; there is more detailed information about the second component in the "notes.dat" file --- MType Morphological type. In some cases, the description "dbl" is used for close binaries --- Stype Spectrum type number=1 Spectrum type: Sy1-Sy2 - Sy galaxy of the corresponding type Sy3 - LINER QSO - quasar BL - lacertides SB - star-burst galaxies HII - extragalactic HII region e - emission spectrum galaxy a - absorption spectrum galaxy The two last notations have been used when there was no necessary information about their spectra. --- Ddia Diaphragm size. When the are several diaphragms, the largest one is presented arcsec Vmag Vmagnitude mag B-V B-V colour index mag U-B U-B colour index mag r_Vmag References for UBV photometry (See "refs.dat" file) --- Var A 'v' indicates optical variability --- F12um IRAS flux at 12 {mu}m number=2 IRAS version 1 Jy l_F25um Limit flag on F25um --- F25um IRAS flux at 25 {mu}m number=2 IRAS version 1 Jy l_F60um Limit flag on F60um --- F60um IRAS flux at 60 {mu}m number=2 IRAS version 1 Jy l_F100um Limit flag on F100um --- F100um IRAS flux at 100 {mu}m number=2 IRAS version 1 Jy *Comments on table7.dat Mrk Markarian designation number --- Sp2 Spectral type --- Mag2 Magnitude of secondary mag z2 Redshift of secondary --- Text Text of note --- *Deleted Survey objects Name Mrk galaxy number --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Mobs Observed magnitude from the CGCG mag n_Mobs An '*' indicates that there were no value in CGCG and that the magnitude given is the original estimates of the authors --- Sp Spectral type --- Nref Reference number (See "refs.dat" file) --- Spect. Spectrum --- Common names Mrk Markarian galaxy number --- Name Other names --- Finding list of common names Name Galaxy name number=1 CG: Case I: IC KUG: Kiso N: NGC U: UCG I Zw: Zw --- Mrk Markarian galaxy designation --- FBS objects by number Mrk Markarian designation number --- Name Name composed with HHMM+DD (hours and minutes of RA 1950, degrees of DE 1950). This name is not unique among FBS galaxies --- Reference codes Nref Reference number --- Ref References --- descrip.doc Description of the FBS Patricia Bauer, Francois Ochsenbein CDS 1997 Oct 20 UNKNOWN UNKNOWN * 28-Aug-1994: The catalogue was provided by courtesy of V.Lipovetskii to H.Andernach; it was numbered A138 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors". The documentation was written by Koichi Nakajima (CDS, and Japanese Data Centre) * 23-Jan-1995: documentation standardized by Patricia Bauer [CDS] * 20-Oct-1997: file refs.dat rewritten by Francois Ochsenbein [CDS] VII_172.xml A Catalogue of Seyfert Galaxies 7173 VII/173 Catalogue of Seyfert Galaxies A Catalogue of Seyfert Galaxies V A Lipovetsky S I Neizvestny O M Neizvestnaya Comm. SAO USSR 55 ??? ??? 1988 1988SoSAO..55....5L Galaxies, Seyfert Magnitudes, absolute Redshifts A list of 959 Seyfert galaxies whose data were obtained up to the beginning of 1987 is compiled. Coordinates, redshifts, UBVR-photoelectric magnitudes, absolute magnitudes, morphological types, fluxes in H and [OIII] 5007, JHKLN-fluxes, far-infrared (IRAS) fluxes, radio-fluxes at 6 and 11 centimeters, monochromatic X-ray fluxes in 0.3-3.5 and 2-10 keV and some other data are presented in six Tables. This Catalogue data may be used as basic ones for some statistical investigations. References contain 957 entries.
General list of objects IAU IAU name --- m_IAU Multiplicity index on IAU name --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec z0 Galactocentric redshift --- r_z0 Redshift reference --- Type Seyfert type --- n_Type Note on Seyfert type number=1 : = probable Sy type ? = uncertain entries of Sy galaxies * = nucleus of bright galaxy with Sy feature --- r_Type Seyfert type reference --- Bmag B magnitude mag r_Bmag B magnitude reference --- E(B-V) Galactic reddening --- BmagAbs Absolute B magnitude mag Morphological and photoelectric data IAU IAU name --- m_IAU Multiplicity index on IAU name --- Mtype Morphological type --- Memb Membership number=1 CL - a member of a cluster of galaxies; GR - a member of a group of galaxies; PA - a member of a pair of galaxies; GR/CL - it is reported in literature about SyG belonging to a cluster, which is studied not sufficiently well and there is no concrete information about its richness. Possible membership is noted ":" --- MajDiam Isophotal major diameter arcmin u_MajDiam Uncertainty flag on MajDiam --- b/a Axis ratio --- u_b/a Uncertainty flag on a/b --- Ref Data reference or finding chart reference --- Aper Aperture diameter of photoelectric measurements arcmin Vmag V magnitude mag U-B U-B colour index mag B-V B-V colour index mag V-R V-R colour index mag u_V-R Uncertainty flag on V-R --- r_Vmag Reference for UBV photometry --- Different spectral range fluxes (X-ray, optics, IR, radio) IAU IAU name --- m_IAU Multiplicity index on IAU name --- l_Xhard Limit flag on Xhard --- Xhard Hard X-ray monochromatic flux (2-10keV or 2-6keV region) uJy n_Xhard ':' for uncertainty, 'V' for variable --- r_Xhard Reference for Xhard --- l_Xsoft Limit flag on Xsoft --- Xsoft Soft X-ray monochromatic flux (0.4-4.5keV or 0.3-3.5keV) in 10-29erg/cm2/s/Hz uJy r_Xsoft Reference for Xsoft --- l_Hbeta Limit flag on Hbeta --- Hbeta Hbeta-line flux in 10-29erg/cm2/s/Hz mJy l_O/H Limit flag on O/Hbeta --- O/H Nebular(5007A[OIII])/Hbeta ratio --- n_O/H ':' for uncertainty, 'V' for variable --- r_HFlux References for H-line flux and O/H ratio --- JFlux Flux in Johnson J band number=1 When the data published included measurements of the object obtained with several apertures, we give those obtained with the maximum one. mJy HFlux Flux in Johnson H band number=1 When the data published included measurements of the object obtained with several apertures, we give those obtained with the maximum one. mJy KFlux Flux in Johnson K band number=1 When the data published included measurements of the object obtained with several apertures, we give those obtained with the maximum one. mJy r_JFlux References for J,H,K- fluxes --- l_LFlux Limit flag on LF --- LFlux Johnson L-band or 3,5m-band flux mJy r_LFlux L-flux reference --- l_NFlux Limit flag on NF --- NFlux Johnson N-band (10m-band) flux mJy r_NFlux N-flux reference --- l_F6cm Limit flag on F6cm --- F6cm 6-cm radio flux (or 7.6 or 8.2cm) Jy n_F6cm * indicates that F6cm contains 7.6cm flux # indicates that F6cm contains 8.2cm flux --- r_F6cm 6-cm flux references --- l_F11cm Limit flag on F11cm --- F11cm 11-cm radio flux (or 21, 31 or 73cm) Jy n_F11cm # means that F11cm contains 21cm flux + means that F11cm contains 31cm flux * means that F11cm contains 73cm flux --- r_F11cm 11-cm flux references --- Far-infrared fluxes IAU IAU name --- m_IAU Multiplicity index on IAU name --- l_F12 Limit flag on F12 --- F12 Far IR flux at 12 {mu}m Jy l_F25 Limit flag on F25 --- F25 Far IR flux at 25 {mu}m Jy l_F60 Limit flag on F60 --- F60 Far IR flux at 60 {mu}m Jy l_F100 Limit flag on F100 --- F100 Far IR flux at 100 {mu}m Jy List of common names IAU IAU name --- m_IAU Multiplicity index on IAU name --- Name Other names --- Finding list of common names Name Name --- IAU IAU name --- u_IAU uncertainty flag on IAU name --- Patricia Bauer CDS 1995 Jan 24 VII_173.xml A catalog of morphological types in 55 rich clusters of galaxies 7174 VII/174 Catalog of morpho. types in 55 rich clusters of gal. A catalog of morphological types in 55 rich clusters of galaxies A Dressler Astrophys. J. Suppl. Ser. 42 565 1980 1980ApJS...42..565D Galaxies, photometry Clusters, galaxy galaxies: clusters: general galaxies: photometry galaxies: structure Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.
Morphological types in 55 rich clusters of galaxies Cluster Cluster name --- Galaxy Galaxy number in the cluster --- X X position mm Y Y position mm RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Mtype Morphological type --- mvis Estimated total apparent magnitude mag mbulge Estimated bulge magnitude number=1 m_V_ =~ -19 - mb/2 mb = -1 means no bulge mb = -2 means indeterminate mag Eps Estimated ellipticity number=2 e = -2 means indeterminate --- Patricia Bauer CDS 1995 Jan 30 VII_174.xml The Edinburgh-Durham southern galaxy catalogue - IV. The cluster catalog 7175 VII/175 Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. The Edinburgh-Durham southern galaxy catalogue - IV. The cluster catalog S L Lumsden R C Nichol C A Collins L Guzzo Mon. Not. R. Astron. Soc. 258 1 1992 1992MNRAS.258....1L J/MNRAS/274/1071 : Edinburgh-Milano cluster redshift survey (Collins+ 1995) The papers of this series are as follows: Paper I: MNRAS 236, 7p (1988) "First results on the galaxy angular correlation function" Paper II: MNRAS 238, 379 (1989) "Image classification and galaxy number counts" Paper III: MNRAS 254, 295 (1992) "w(theta) from the full survey" Paper V: MNRAS 255, 21p (1992) "The cluster correlation function" Paper VI: MNRAS 265, 867 (1993) "The stability of w(theta)" The EDSGC is not yet published in these papers. Clusters, galaxy catalogs galaxies: clusters: general We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaxy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.
the Edinburgh-Durham cluster catalogue EDCC sequential EDCC cluster identification number --- u_EDCC uncertainty flag on EDCC, indicating that such clusters could not be distinguished from the surrounding field (see paper, p6R) --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec M1 magnitude of first brightest member mag M3 magnitude of third brightest member mag M10 magnitude of tenth brightest member mag u_M10 uncertainty flag of M10 where the visual inspection gave a clearly different result (see paper, p6R) --- Nclus number of galaxies within the Abell radius between M3 and M3+2 "after" the background galaxies have been removed ct u_Nclus uncertainty flag of Nclus (see u_M10) --- Nback number of background galaxies within the same radius to the same magnitude limit (see Nclus, and paper p6R) ct THA Abell radius deg F character 'F' for field number --- FIELD Schmidt J survey field number --- RUN1 number of times the cluster was located in run 1 (see paper p2) ct RUN2 the above in run 2 ct RUN3 the above in run 3 ct DEB 'd'= the cluster was deblended, ' '= not --- ACO Abell identification number (see paper p6R) number=1 ACO-identifications in the last column were aligned and brackets converted to a ':' sign AFTER the cluster number. -- H.A. 22-Oct-1992 --- u_ACO only the clusters' Abell radii overlap number=1 ACO-identifications in the last column were aligned and brackets converted to a ':' sign AFTER the cluster number. -- H.A. 22-Oct-1992 --- Koichi Nakajima CDS 1994 Mar 11 UNKNOWN UNKNOWN The catalogue was provided by courtesy of R.C.Nichol to H. Andernach; it was numbered A144 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" VII_175.xml Spectroscopy and Photometry of Elliptical Galaxies. VI. Sample Selection and Data Summary. 7176 VII/176 Photometry and Spectroscopy of Elliptical Galaxies Spectroscopy and Photometry of Elliptical Galaxies. VI. Sample Selection and Data Summary. S M Faber G Wegner D Burstein R L Davies A Dressler D Lynden-Bell R J Terlevich Astrophys. J. Suppl. Ser. 69 763 1989 1989ApJS...69..763F Clusters, galaxy Photometry Redshifts galaxies: clusters: general galaxies: photometry galaxies: distances and redshifts Photometric and spectroscopic data are presented for a survey of the nearest and brightest elliptical galaxies. Distances, velocities relative to the cosmic rest frame, and residual velocities relative to a velocity-flow model are calculated for individual galaxies and groups. Information is provided on the selection and completeness of the target and observed samples. Both samples appear to be noticeably deeper in the north than in the south. A new diameter system for ellipticals is described that is easy to measure on survey prints and is a useful indicator of B_T_ magnitude. Important Notices: * This catalog is NOT the same with that of printed, but is selected. The original explanation file "a149.doc" from Burstein to Andernach describes as follows: "This file contains a total of 483 galaxies having relatively accurate Dn values (quality parameter 2 or better). Of these 483 galaxies, 385 were used by Lynden-Bell et al. for studies of the velocity field. The reasons why the 71 galaxies were excluded from the final survey are detailed in Lynden-Bell et al., and range from absence of velocity dispersions, a lower limit on velocity dispersions, and a surface brightness limitation." * However, the resultant number of galaxies by above elimination is 479, so the number of records in this file is 479. * In Lynden-Bell et al. (1988ApJ...326...19L), the following description is seen (p25L) "Of them, 433 have measured velocity dispersions. Galaxies with velocity dispersions less than 100 km/s ... eliminated all 25 of them from final data set. ... (8 more galaxies are eliminated due to various reasons)." The number of those galaxies which have no velocity dispersion measurement (0.000 is written in "logSIG" column) is 46, hence "71" (=46+25) as above. The number 400 (=479-71-8) coincides with that written in the top line of the Abstract of Lynden-Bell et al. Therefore, the number of "483" written above seems to be erroneous. The number "385" is seen in the Fig.1 of Lynden-Bell et al. * The values in column "B-V0" in the file "table1" are those corrected according to the ERRATA (ApJS, 71,173 (1989)). * Columns "n_{B-V}", "D_{FW}", "R_{FW}", "k", "M" and "Remarks" in the published Table 1 are omitted in the file. * The blank entries in the published Table 1 is filled, in this file, by some unexpected values, such as 0 in columns "Ngr", "Vhel", "Vgr", "B-V0", "SBe", "logSIG", "Mg2", or 0.10 in "BT", -0.99 in "logAe". * The relevant data have been corrected for extinction, redshift and cosmological effects, and "logSIG" and "Mg2" are corrected for distance-dependent aperture effects, as detailed in Davies et al. (1987ApJS...64..581D). * For some columns of Table 1, detailed explanations are given in the paper. In the following "Byte-by-byte Description...", they are indicated by the page number (e.g., p765L).
Photometric and spectroscopic obs. data for elliptical galaxies NO galaxy ID number in this survey number=1 In the published Table 1, the consecutive number is given here. However, the archived file is not consecutive because of the reason written in the Notes of Description above. See paper p765L. --- Name Galaxy name: 'N'=NGC, 'I'=IC, 'U'=UGC 'E&G'=ESO, 'CR'=Chincarini & Rood(1971), 'A'=anonymous, 'D'=Dressler(1980) number=2 the abbreviations are: 'N'=NGC, 'I'=IC, 'U'=UGC 'E&G'=ESO, 'A'=anonymous, 'CR'=Chincarini & Rood (1971ApJ...168..321C), 'D'=Dressler (1980ApJS...42..565D); the descriptions "Dressler (1983)" in the paper should be read "Dressler (1980)", both in text and in references. --- GLON galactic longitude deg GLAT galactic latitude deg AB galactic extinction in B magnitude. p765R mag Ngr number of group to which galaxy is assigned. p765R --- Vhel observed heliocentric velocity of galaxy. p765R km/s Vgr heliocentric velocity for group. p765R km/s B-V0 average B-V color in 67" diameter aperture number=3 This is not that in Table 1, but the true one as described in ERRATA (ApJS, 71,173 (1989)) mag BT Total magnitude on the RC2 system from fitting to the photoelectric aperture growth curve. mag logAe =-0.99 de Vaucouleurs effective diameter expressed as log(Ae/0.1arcmin). p765R 0.1arcmin q_logAe quality flag for Ae and SBe. p765R --- q_logDn quality flag for Dn. p765R,p777L --- q_BT quality flag for BT. p765R,p777L --- SBe mean B surface brightness within Ae. mag/arcsec2 logDn angular diameter, "Dn", expressed as log(Dn/0.1arcmin). p765R 0.1arcmin logSIG rest-frame nuclear velocity dispersion, "SIG", expressed as log(SIG). p777L km/s Mg2 nuclear Mg2 index, fully corrected. p777L mag Koichi Nakajima CDS 1994 Feb 15 UNKNOWN UNKNOWN * The catalogue was provided by courtesy of D.Burstein to H. Andernach; it was numbered A149 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" * 14-Mar-1994: First archived (Koichi Nakajima [CDS]) (The date of the latest archiving, see the date of each file.) VII_176.xml A Compilation of Redshifts and Velocity Dispersions for Abell Clusters (epoch 1991.2) 7177 VII/177 Redshifts and Vel Dispersions for Abell Clusters A Compilation of Redshifts and Velocity Dispersions for Abell Clusters (epoch 1991.2) M F Struble H J Rood ApJS 77 363 1991 1991ApJS...77..363S Clusters, galaxy Redshifts The catalog presents a list of redshifts for 758 Abell clusters, and velocity dispersions for 121, published as of 1991 March. We present another list of 33 Abell clusters with published redshifts, most of which are probably redshifts of foreground or background galaxies superposed on, or near, the Abell clusters. Over the past 4 years, the published number of redshifts of member galaxies in clusters increased by a factor of 2.0, but the number of cluster redshifts increased by only a factor of 1.3, while the number of cluster velocity dispersions derived from 50 or more redshifts of member galaxies increased by a factor of 3.8 (from 6 to 23).
Redshifts and velocity distribution for Abell clusters Abell Abell number --- Abell_mem * denotes membership in Abell's non- statistical sample. --- n_Abell suffix to Abell number (see paper, p363R-p364L) --- RAh Right ascension (B1950) of the cluster center (hours) h RAm right ascension (minutes) min DE- declination sign (B1950) --- DEd declination of the cluster center (degrees) (B1950) deg DEm declination (minutes) arcmin Zadt adopted z --- l_Nadt limit flag of Nadt --- Nadt number of galaxies used to determine Zadt (see paper, p364) ct SIGadt adopted sigma in the rest frame of cluster (see paper, p364) km/s NOTE note (see below) 'a'= note in Sarazin et al. 1982; 'b'= note in Fetisova 1982; 'c'= remarks given in the paper pp375-376; 'd'= a, b & c; 'e'= a & b; 'f'= a & c; 'g'= b & c. --- Zsr1 adopted z listed in SR1 The "SR1" denotes the authors' previous paper (Astrophys. J. Suppl. 63, 543 (1987)), which is archived as catalog VII/95. --- l_Nsr1 limit flag of Nsr1 --- Nsr1 number of redshifts used to determine Zsr1 ct SIGsr1 adopted sigma determined from references in SR1 km/s Znew z from a source more recent than, or not contained in SR1 --- l_Nnew limit flag of Nnew --- Nnew number of redshifts used to determine Znew (see paper, p364) ct SIGnew sigma determined from redshifts of cluster members contained in the new references in r_Znew km/s r_Znew code for reference source of the data in Znew, Nnew, and SIGnew (for code >= 71 see "refs" file, for code < 71 see SR1) --- reference list for the table Ref_num Reference number The present data supersede the former "SR1". However, the present list of references follows that in "SR1", beginning its number from 71. For the code number less than 71, see "SR1". --- Ref Reference information --- James E. Gass SSDOO/ADC 1997 Oct 15 UNKNOWN UNKNOWN The raw files were provided by the author H.J. Rood to H. Andernach and have been edited by H. Andernach and E.A. Stengler-Larrea to match the published version. It was numbered A121 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors". 08-Nov-1993: First archived in J/ApJS/77/363/, without "refs". 14-Feb-1994: Moved to VII/177/, appending the file "refs". (The date of the latest archiving, see the date of each file.) 15-Oct-1997: Standardized the ReadMe document using Intro file, etc. VII_177.xml An Optical Catalog of Extragalactic Emission-line Objects Similar to Quasistellar Objects 7178 VII/178 Optical Cat of Extragalactic Emission-line Obj An Optical Catalog of Extragalactic Emission-line Objects Similar to Quasistellar Objects A Hewitt G Burbidge Astrophys. J. Suppl. Ser. 75 297 1991 1991ApJS...75..297H Active gal. nuclei A catalog of 935 galaxies which have optical properties similar to those of QSOs is given. A subsidiary table of cross-identifications enables the reader to relate the name of a given object to its coordinate name. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z =< 0.2, and have mostly been classified as Seyfert galaxies, N systems, or radio galaxies. The Hubble diagram for all of the objects with z =< 0.2 is shown. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z > 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06.
Optical catalog of extragalactic emission-line objects similar to quasi-stellar objects (935 galaxies) CONAME Coordinate designation name number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies --- NAME Other names of the object number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies --- RAh Right Ascension 1950 (hours) number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies h RAm Right Ascension 1950 (minutes) number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies min RAs Right Ascension 1950 (seconds) number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies s DE- Declination 1950 (sign) number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies --- DEd Declination 1950 (degrees) number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies deg DEm Declination 1950 (minutes) number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies arcmin DEs Declination 1950 (seconds) number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies arcsec mv Apparent magnitude; V mag. when available number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies mag Zem emission redshift number= For any given object, multiple values of columns "NAME", "REF1" and "REF2" are given on multiple lines, while only one value of each of the the other columns is given (on the first line of data). number= Statistics on table1.dat: 935 objects 700 objects with redshifts less than 0.02, remainder are objects with much higher redshifts, predominantly powerful radio galaxies --- u_Zem when Zem was within parenthesis (?) number=1 The meaning of u_Zem is not given in the paper. --- REF1 source of Zem, or object type number=2 The first line of data for an object gives 'z' for column 'REF1' if REF2 is the source of Zem. The second line of data gives an abbreviated expression of object type, as follows: sy : Seyfert galaxy sy1: Seyfert 1 sy2: Seyfert 2 rg : Radio galaxy n : Compact galaxy (see Morgan 1958; Matthews, Morgan, and Schmidt (1964) e : Emission lines present but not necessarily strong we : Weak emission lines me : Moderate emission Lines se : Strong emission lines See Smith, Spinrad, and Smith (1796) for more information concerning the use of e, we, me, and se to characterize the optical spectra of radio galaxies. --- REF2 reference code number of Zem or type number=2 The first line of data for an object gives 'z' for column 'REF1' if REF2 is the source of Zem. The second line of data gives an abbreviated expression of object type, as follows: sy : Seyfert galaxy sy1: Seyfert 1 sy2: Seyfert 2 rg : Radio galaxy n : Compact galaxy (see Morgan 1958; Matthews, Morgan, and Schmidt (1964) e : Emission lines present but not necessarily strong we : Weak emission lines me : Moderate emission Lines se : Strong emission lines See Smith, Spinrad, and Smith (1796) for more information concerning the use of e, we, me, and se to characterize the optical spectra of radio galaxies. --- References to Table 1 by reference number References to Table 1 in alphabetical order Ref Reference number --- dot --- Text Reference text --- Gail L. Schneider (mod. G.A. Reichert) SSDOO/ADC 1997 Jul 03 UNKNOWN UNKNOWN The catalogue was provided by the author A.Hewitt to H. Andernach; it was numbered A122 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors". Three differences were found between the "table1.dat" file and the Table 1 of the published version of the paper. The differences were corrected in the electronic file to agree with the published table. It is possible that some differences still remain. 24-Nov-1993: First archived in J/ApJS/75/297/. 14-Feb-1994: Seconds of the declination of 0003-503 corrected Moved to VII/178/. (For the most recent archive date, see the date of each file.) VII_178.xml Kiso survey for ultraviolet-excess galaxies. XVIII (KUG18) 7179 VII/179 Kiso Survey for UV-Excess Galaxies. XVIII Kiso survey for ultraviolet-excess galaxies. XVIII (KUG18) B Takase N Miyauchi-Isobe Publ. Natl. Astron. Obs. Japan, Vol. 3 169 1993 1993PNAOJ...3..169T Galaxies, UV-excess Surveys The already published catalogue series I - XVII of the KUGs (Kiso Ultraviolet- excess Galaxies) has now covered the sky area of some 5,100 square degrees. The number of the KUGs detected is in total 8,968, giving the number density of 1.8 per square degree. After deleting the objects which appear repeatedly in some neighbouring survey areas, the net count of the KUGs results in 8,162. This may be an appropriate sample number for making some statistical study of the KUG, although the sky coverage is not yet sufficient. This catalog presents a merged version of the 17 catalogues, where all KUGs are arranged in order of the right ascension, for the convenience of users.
The Catalogue of KUG18 KUG KUG name composed of the values of right ascension and declination, with a suffix --- RAh right ascension (hours) (B1950) number=1 RA and DE are determined by the method by Noguchi et al.(1980) (see references of the paper). h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination (degrees) (B1950) number=1 RA and DE are determined by the method by Noguchi et al.(1980) (see references of the paper). deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec TYPE Morphological type number=2 The classification scheme by Takase et al.(1983) is as follows: IC: Irregular with clumsy HII regions Ig: Irregular with a conspicuously giant HII region Pi: Pair of interacting components Pd: Pair of detached components Sk: Spiral with knots of HII regions along arms Sp: Spiral with peculiar bar and/or nucleus C: Compact ?: Unclassifiable --- u_TYPE ':'= the type is not so certainly assigned --- Amaj Major diameter of image number=3 The diameters are roughly measured on the Palomar Sky Survey blue print. arcmin X sign of multiplication --- Amin Minor diameter of image number=3 The diameters are roughly measured on the Palomar Sky Survey blue print. arcmin Mapp Apparent magnitude number=4 Apparent magnitude without ':' is that taken from other catalogues of which names are given in the last column of the original I - XVII catalogues. That with ':' is the roughly estimated one on the Palomar Sky Survey blue print. mag u_Mapp ':'= uncertain magnitude number=4 Apparent magnitude without ':' is that taken from other catalogues of which names are given in the last column of the original I - XVII catalogues. That with ':' is the roughly estimated one on the Palomar Sky Survey blue print. --- UVX Degree of UV excess number=5 'H'=high, 'M'=medium, 'L'=low. See Takase et al.(1983). --- n_INDEX '*'= note is given in the Table of the paper number=6 '*' denotes those KUGs detected repeatedly. These have more than two indices, among which the first appearance is shown in this catalogue. The indices corresponding to the later appearances are indicated in the "Notes" column of the Table of the paper. --- INDEX Index composed as follows: 'C'+ 2-figures = catalogue volume number 'A'+ 4-figures = area number last 3-figures = galaxy number in the area --- NAME Names given in other catalogues number=7 The abbreviated notations used here have the following correspondence to those adopted in MOL (Dixon and Sonneborn, 1980): A:ARP, H:HARO, I:IC, M:MCG, MK:MKG, N:RNGC, U:UGC, V:Vorontsov-Velyaminov (1977), Z:ZWG, nZ:nZW(n=1,2,...,8). --- Koichi Nakajima CDS 1994 Jan 24 UNKNOWN UNKNOWN * This catalogue supersedes VII/150. * References of previous publications: I. Annals Tokyo Astron. Obs., II Ser., Vol. 19, No. 4, p 595, 1984 II. Annals Tokyo Astron. Obs., II Ser., Vol. 20, No. 3, p 237, 1985 III. Annals Tokyo Astron. Obs., II Ser., Vol. 20, No. 4, p 335, 1985 IV. Annals Tokyo Astron. Obs., II Ser., Vol. 21, No. 1, p 127, 1986 V. Annals Tokyo Astron. Obs., II Ser., Vol. 21, No. 2, p 181, 1986 VI. Annals Tokyo Astron. Obs., II Ser., Vol. 21, No. 3, p 251, 1987 VII. Annals Tokyo Astron. Obs., II Ser., Vol. 21, No. 4, p 363, 1987 VIII. Annals Tokyo Astron. Obs., II Ser., Vol. 22, No. 1, p 41, 1988 IX. Publ. Natl. Astron. Obs. Japan, Vol. 1, No. 1, p 11, 1989. X. Publ. Natl. Astron. Obs. Japan, Vol. 1, No. 2, p 97, 1989. XI. Publ. Natl. Astron. Obs. Japan, Vol. 1, No. 3, p 181, 1990. XII. Publ. Natl. Astron. Obs. Japan, Vol. 2, No. 1, p 7, 1991. XIII. Publ. Natl. Astron. Obs. Japan, Vol. 2, No. 1, p 37, 1991. XIV. Publ. Natl. Astron. Obs. Japan, Vol. 2, No. 2, p 239, 1991. XV. Publ. Natl. Astron. Obs. Japan, Vol. 2, No. 3, p 399, 1992. XVI. Publ. Natl. Astron. Obs. Japan, Vol. 2, No. 4, p 573, 1992. XVII. Publ. Natl. Astron. Obs. Japan, Vol. 3, No. 1, p 21, 1993. 06-Jun-1995: standardized this file. (ADC) VII_179.xml Population studies in groups and clusters of galaxies. II. A catalog of galaxies in the central 3.5 degs of the Fornax Cluster 7180 VII/180 Gal in 3.5 Degs of Fornax Cluster, Five Nearby Groups Population studies in groups and clusters of galaxies. II. A catalog of galaxies in the central 3.5 degs of the Fornax Cluster H C Ferguson AJ 98 367 1989 1989AJ.....98..367F Population studies in groups and clusters of galaxies. II. A catalog of galaxies in the central 3.5 degs of the Fornax Cluster H C Ferguson A Sandage AJ 100 1 1990 1990AJ....100....1F Clusters, galaxy Galaxy catalogs This catalog represents the combination of results published in two papers: Ferguson, H.C. 1977 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supercedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_B_T__=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ I8, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_B_T__ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.
Likely Fornax Cluster members FCC Fornax Cluster Catalog number number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- RAh right ascension (hours) (B1950) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) h RAm right ascension (minutes) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) min RAs right ascension (seconds) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) s DE- declination sign number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- DEd declination (degrees) (B1950) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) deg DEm declination (minutes) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) arcmin DEs declination (seconds) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) arcsec Mem membership status of the galaxy 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- MORPH morphological type number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- BT total blue apparent magnitude number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) mag RADef effective radius (arcsec) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) arcsec logD decimal logarithm of the diameter in units of 0.1arcmin at an isophoto number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) 0.1arcmin SOURCE source of coordinates, magnitudes, and effective radii. See paper. number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- Vhel heliocentric velocity (km/s) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) km/s e_Vhel uncertainty of the velocity (km/s) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) km/s r_Vhel source of the velocity 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- Note additional notes on individual galaxies listed in the paper number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- NAME names of the galaxy (up tp 4) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- IAU IAU coordinate designation number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=Richter and Sadler(1985), 2=Jones and Jones(1980), 3=Lauberts(1982) --- Possible members and likely backgr. gal. PREFIX prefix of Fornax Cluster Catalog number indicating the background galaxy number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw --- FCC Fornax Cluster Catalog number number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw --- f_FCC Flag indicates that velocity or alt. name listed in notes for Table 3. number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw --- RAh right ascension (hours) (B1950) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw h RAm right ascension (minutes) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw min RAs right ascension (seconds) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw s DE- declination sign number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw --- DEd declination (degrees) (B1950) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw deg DEm declination (minutes) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw arcmin DEs declination (seconds) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw arcsec Mem membership status of the galaxy 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw --- MORPH Morphological type number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw --- BT total blue apparent magnitude number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw mag RADef effective radius (arcsec) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw arcsec logD decimal logarithm of the diameter in units of 0.1arcmin at an isophoto number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw 0.1arcmin SOURCE source of coordinates, magnitudes, and effective radii. See paper. number= 1=definite member, 2=likely member, 3=possible member, 4=likely background, 5=definite background, 6=likely plate flaw --- Notes to Table 3 (="p2tbl3") PREFIX prefix of Fornax Cluster Catalog number indicating the background galaxy --- FCC Fornax Cluster Catalog number --- Note notes for galaxy designated '*'in Table 3, column 6. Velocity or alternate name. --- Galaxy catalogue in Leo group Galaxy catalogue in Dorado group Galaxy catalogue in NGC1400 group Galaxy catalogue in NGC5044 group Galaxy catalogue in Antlia group N galaxy number number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- PLATE Las Campanas plate ID number (plate) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- HYPH hyphen number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- GAL Las Campanas plate ID number (galaxy) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- RAh right ascension (hours) (B1950) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background h RAm right ascension (minutes) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background min RAs right ascension (seconds) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background s DE- declination sign number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- DEd declination (degrees) (B1950) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background deg DEm declination (minutes) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background arcmin Mem membership class 1=definite member, 2=likely member, 3=possible member, 4=likely background number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- COMM comma (if another membership class follows) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- u_Mem another membership class when class or reality is uncertain number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- BT total B magnitude number= 1=definite member, 2=likely member, 3=possible member, 4=likely background mag AXma major axis in arcsec (eye estimate) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background arcsec AXmi minor axis in arcsec (eye estimate) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background arcsec MORPH morphological type number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- Name alternate name(s) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- Vhel heliocentric (usually) velocity (km/s) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background km/s e_Vhel uncertainty of Vhel number= 1=definite member, 2=likely member, 3=possible member, 4=likely background km/s r_Vhel reference of Vhel number=1 See note 1 of "expl.txt" file. --- r_BT reference of BT number=1 See note 1 of "expl.txt" file. --- Note notes number=2 See note 2 of "expl.txt" file. --- MORPH1 morphological type code number=3 See note 3 of "expl.txt" file. --- CONJ morphological type conjunction number=4 See note 4 of "expl.txt" file. --- MORPH2 alternate morphological type(3) number= 1=definite member, 2=likely member, 3=possible member, 4=likely background --- expl.txt Explanation for format and notes of paperIII Koichi Nakajima CDS James Gass SSDOO/ADC 1997 Jul 29 UNKNOWN UNKNOWN The catalogue was provided by courtesy of H.C. Ferguson to H. Andernach; it was numbered A102 and A112 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 23-Jan-1993: Paper II was archived as VII/160/. 08-Nov-1993: Paper III was archived as J/AJ/100/1/. 14-Mar-1994: Both papers were joined into VII/180/. (The date of the latest archive, see the date of each file.) 29-Jul-1997: ReadMe Document standardized. UNKNOWN UNKNOWN * Tables are not the same with those in the paper. * The format of item 13 in "expl" file is not correct. It is corrected in the Byte-by-byte Description of file, below. * For the series of this paper, [paper I] Astron. J. 96, 1520 (1988) [paper IV] Astron. J. 101, 765 (1991) (There is no catalogue in these papers.) * A similar catalogue of Virgo cluster is in Astron. J. 90, 1681 (1985). VII_180.xml A catalog of X-ray measurements of selected samples of active galaxies and nuclei 7181 VII/181 X-ray of active galaxies and nuclei A catalog of X-ray measurements of selected samples of active galaxies and nuclei R Della Ceca G G C Palumbo M Persic E A Boldt G De Zotti E E Marshall Astrophys. J. Suppl. Ser. 72 471 1990 1990ApJS...72..471D X-ray sources Active gal. nuclei Galaxies, Seyfert QSOs BL Lacertae objects: general galaxies: nuclei galaxies: Seyfert X-rays: galaxies quasars: general X-ray fluxes or upper limits in the 2-10 keV energy band from the HEAO 1 A-2 experiment are given for well-defined samples of QSOs and of Seyfert galaxies of types 1, 1.5 and 2, and for a list of BL Lac objects (334 sources in total). All on-orbit X-ray measurements of these objects published between 1976 and 1986 from other experiments have also been catalogued.
Catalog for PG Quasars Catalog for Seyfert 1 and 1.5 galaxies Catalog for Seyfert 2 galaxies Catalog for BL Lacertae objects RAh Right ascension 1950 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 h RAm Right ascension 1950 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 min RAs Right ascension 1950 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 s DE- Declination sign number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- DEd Declination 1950 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 deg DEm Declination 1950 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 arcmin DEs Declination 1950 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 arcsec Name PG name (Schmidt and Green 1983). For other names see table6 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- z Redshift (Schmidt and Green 1986) number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- Bmag B magnitudes (Schmidt and Green 1983) number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 mag Instr Instrument or experiment by which the measurement was taken. number=1 Instrument or experiment: A-1 : Experiment A-1 aboard HEAO-1 A-2 : Experiment A-2 aboard HEAO-1 A-3 : Experiment A-3 aboard HEAO-1 A-4 : Experiment A-4 aboard HEAO-1 AL/P : Low-Energy Experiment aboard Exosat (Aluminum/Parylene Filter) A5SSI : Ariel-5 Sky Survey Instrument A5MSSL : Ariel-5 Proportional Counter Spectrometer A6 : Ariel-6 B : Low-Energy Experiment aboard EXOSAT (Boron Filter) HRI : High-Resolution Imager aboard the Einstein Observatory IPC : Imaging Proportional Counter aboard the Einstein Observatory LE : Low-Energy Experiment aboard EXOSAT 3LX : Low-Energy Experiment aboard EXOSAT (Thin Lexan Filter) ME : Medium-Energy Experiment aboard EXOSAT MPC : Monitor Proportional Counter aboard the Einstein Observatory OSO-7 : OSO-7 OSO-8 : OSO-8 P/P : Low-Energy Experiment aboard EXOSAT (Polypropylene Filter) SAS-3 : SAS-3 SSS : Solid-State Spectrometer aboard the Einstein Observatory TGSPC : Gas-Scintillation Proportional Counters aboard TENMA UHU : UHURU --- E1 Lowest value of the spectral window number=3 spectral window of observation: The reader is cautioned, however, that the quoted spectral window does not always match the energy band over which the photons were actually detected. If one single energy value is reported, the measurement is monochromatic at that energy. For some EXOSAT Low-Energy Experiment measurements, only filters are reported in column Instr. The relative spectral windows are still poorly defined and may undergo revisions hence are not reported in this column keV n_E1 A '-' indicates the spectral window number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- E2 Highest value of the spectral window (E1_E2) when n_E = '-' number=3 spectral window of observation: The reader is cautioned, however, that the quoted spectral window does not always match the energy band over which the photons were actually detected. If one single energy value is reported, the measurement is monochromatic at that energy. For some EXOSAT Low-Energy Experiment measurements, only filters are reported in column Instr. The relative spectral windows are still poorly defined and may undergo revisions hence are not reported in this column keV Note Note (MED1.05 for flux MKN 421, A5SSI) number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- l_Flux Limit flag on flux number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- Flux Flux measured in the energy band E1-E2 or monochromatic at a given energy, according to column E1-E2 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- n_Flux A '-' indicates an interval of flux number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- Flux2 Higest value of flux interval when n_Flux = '-' number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- u_Flux Uncertainty flag on flux interval number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- e_Flux Rms uncertainty on Flux number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- u_e_Flux Uncertainty flag on e_flux number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- x_Flux Units in which the quantities reported in the two previous columns are measured. number=2 Units of Flux: CTCQS : counts/cm2/s CTS/S : counts/s KCQSK : keV/cm2/s/keV PCQS : photons/cm2/s PCQSK : photons/cm2/s/keV PH/S : photons/s Jy : Jansky R15 : R15 Counts --- l_Flux0 Limit flag on Flux0 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- Flux0 Flux from reference in column ref. If the flux in column E1 is monochromatic the physical units here will be mW/m2/Hz number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 mW/m2 n_Flux0 A '-' indicates an interval of flux number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- Flux02 Highest value of flux interval when n_Flux0= '-' number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- u_Flux0 Uncertainty flag on flux interval number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- e_Flux0 Rms uncertainty on Flux0 or upper limit of error on Flux0 if n_e_Flux0='-' (in units of Flux0) number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 mW/m2 n_e_Flux0 A '-' indicates an interval uncertainty on Flux0 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- e(Flux0)l Error on Flux0 (lower limit) number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 mW/m2 ref. Number codes to references, explained in file "ref.num" number=4 If for a given measurement more than one code are quoted, the first code refers to the original paper from which the measurement quoted in table2 is taken. The following code(s) refer to paper(s) where the same measurement is quoted and discussed. Such references are reported here in order to provide more complete information. While special care was devoted to finding original measurements, no completeness is claimed on subsequent publications dealing with the same measurement. --- A-2 A-2 flux measured in R15 counts number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- n_A-2 The flags "c" and "L" indicate contamination from a nearby bright X-ray source and low galactic latitude (|b|<20 deg), respectively. number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- e_A-2 Rms uncertainty on A-2 number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 --- ObsTime Average observation time (in days of the year 1977) during the first six-month all-sky survey completed by the HEAO-1 spacecraft number= For NGC 4151 (table3): reported in reference 15 there are also the fluxes of NGC 4151 obtained interpolating the counts with different spectra. Measurements around 100 Kev for NGC 4151 have been collected in reference 80 d Other names of PG Quasars Other names of Seyfert 1 and 1.5 galaxies Other names of Seyfert 2 galaxies Other names of BL Lac objects Note See note number=1 * = Sources classified as Seyfert 1 by Cheng et al., 1985 They are also present in the Seyfert 1 and 1.5 lists (tables 3 and 7) C = Sources classified as Seyfert 1 by Cheng et al., 1985 C1.5 = Sources classified as Seyfert 1.5 by Cheng et al., 1985 E = Seyfert 1 from Edelson, 1987 E2 = This source has been classified as Seyfert 2 by Edelson, 1987, but as Seyfert 1.5 by Cheng et al., 1985 It is included only in the Seyfert 1 and 1.5 lists (tables 3 and 7) F = Seyfert 1 from Fairall, 1986 + = Sources classified as Quasars by Schmidt and Green, 1983 They are also present in the Quasar lists (tables 2 and 6) D = This source has been classified as Seyfert 2 by Edelson, 1987 V = From Veron-Cetty,and Veron, 1987, BLLac list B = From Burbridge,and Hewitt, 1987 Vq = From Veron-Cetty,and Veron, 1987, Quasars list --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Opt. Names from optical catalogues --- Radio Names from radio catalogues --- X-ray Names from X-ray catalogues --- IRAs IRAS name from positional coincidence --- Koichi Nakajima, Patricia Bauer CDS 1994 Jun 23 UNKNOWN UNKNOWN The files were forwarded to CDS by Heinz J. Andernach (courtesy G. Palumbo) VII_181.xml A wide-field multicolor survey for high-redshift quasars, z>=2.2 . I. Photometric catalog and survey selection function 7182 VII/182 Cat of High-Redshift Quasars, z >= 2.2, in SGP and F401 A wide-field multicolor survey for high-redshift quasars, z>=2.2 . I. Photometric catalog and survey selection function S J Warren P C Hewett M J Irwin P S Osmer Astrophys. J. Suppl. Ser. 76 1 1991 1991ApJS...76....1W A wide-field multicolor survey for high-redshift quasars, z>=2.2 . I. Photometric catalog and survey selection function S J Warren P C Hewett P S Osmer Astrophys. J. Suppl. Ser. 76 23 1991 1991ApJS...76...23W Galaxy catalogs QSOs (Paper I) We provide details of a multicolor ( u, b_j_, v, or, r, i), wide-field, faint magnitude survey for high-redshift (z >= 2.2 ) quasars. The survey extends over the magnitude range 16 <= m_or_ <= 20 and covers a total area of 58.6 square degrees. Sources of incompleteness in the photometric catalog are quantified, giving the survey an effective area of 45.7 square degrees. Particular attention is paid to the details of the plate-matching and image-classification procedures used in the generation of the photometric catalog from which quasars are selected, in order that the number of spurious quasar candidates be kept to an absolute minimum. The selection of candidates incorporates a number of novel features, including treating the multicolor information as low-resolution spectra, adopting a quantitative candidate identification algorithm that employs all the available information, and requiring only that objects be detected in the or passband. We describe how model quasar spectra are used to calculate the selection function for the survey, and we present the computed sample completeness, as a function of redshift and magnitude, for a range of representative quasar types. The spectroscopic results of the survey are reported in a companion paper and the derivation of the quasar luminosity function at high redshift will be reported in a third paper. (Paper II) In a wide-field multicolor survey (45.7 deg^2^, 16.0 <= m_or_ <= 20.0) we have discovered 130 new quasars, of which 100 are of redshift z >= 2.2. There are 49 new quasars of redshift z >= 3.0 including three of z >= 4.0. We provide spectra, coordinates, redshifts, broad-band magnitudes (u, b_j_, v, or, r, i), line-equivalent widths for Lyman-{alpha}/N_V and C_IV, FWHM C_IV, and continuum spectral indices for all the new quasars. The sample includes 96 quasars selected according to the rigid criteria detailed in the companion paper by Warren, Hewett, Irwin, and Osmer. These are combined with 14 previously known quasars in one of our fields, which also meet these selection criteria, to form a complete sample. The median equivalent width for Lyman-{alpha}/N_V for the complete sample is 67A, and for C_IV is 31A. The median FWHM C_IV is 35A and the median spectral index is {alpha} = -0.60. The complete sample contains at least five broad absorption-line quasars. We have obtained spectra of a total of 473 multicolor-selected candidates. The proportion of quasars found, including previously-known quasars, of all redshifts, is 30%. The proportion of quasars of redshift z >= 2.2 in the list of candidates that satisfy the selection criteria of the complete sample is 43%. Finally we limit the sample to the 85 objects of redshift z >= 2.2 in the complete sample, and summarize the relevant observational data input to the calculation of the luminosity function, comprising the redshift versus magnitude distribution and the distribution of the spectral properties. The analysis of the luminosity function will be presented in a forthcoming paper. * For paper II, see also documentation files "doc.tex" (LaTeX) or "doc.txt" (plain ascii).
high-z QSOs in SGP and F401 (II) Note 'n' is there is a note --- ID ! Name based on 1950 coordinates Notes on individual quasars # 0043-296 is also in Boyle et al. 1990 and Anderson et al., 1991. # 0043-275 redshift incorrectly stated in Warren et al. 1987a. # 0049-286 is also in Anderson et al. 1991. # 0052-297 is also in Anderson et al. 1991. # 0100-283A is classified as marginally non-stellar. # 0100-292 is fainter than the sample limit. # 0101-304 spectral index taken from Schneider, Schmidt, & Gunn 1989. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- ! Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec DATEy UT date of observation: year a DATEm UT date of observation: month --- DATEd UT date of observation: day d TEL ! Telescope where spectrum obtained: A = AAT, C = CTIO 4 m. --- z Redshift --- u_z Uncertainty flag for z --- ListA "Y" if object included in List A --- ListB "Y" if object included in List B --- Plot ! Plot number in Figure 1 (SGP) and Figure 2 (F401) (see paper) --- l_m(u) Limit flag (>) on m(u) --- m(u) Magnitude in broad-band UKST band mag l_m(bj) Limit flag (>) on m(bj) --- m(bj) Magnitude in broad-band UKST band mag l_m(v) Limit flag (>) on m(v) --- m(v) Magnitude in broad-band UKST band mag m(or) Magnitude in broad-band UKST band mag m(r) Magnitude in broad-band UKST band mag l_m(i) Limit flag (>) on m(i) --- m(i) Magnitude in broad-band UKST band mag W(Ly1) Equivalent width Lyman-{alpha}/NV blend 0.1nm u_W(Ly1) Uncertainty flag (:) on W(Ly1) --- W(CIV) Equivalent width (BAL emission) of CIV line 0.1nm u_W(CIV) Uncertainty flag (:) on W(CIV), or dash (EM eq. width exists), or blank --- WEM(CIV) Equivalent width (EW emission) of CIV line 0.1nm e_W(CIV) FWHM of W(CIV) 0.1nm u_e_W(CIV) Uncertainty flag (:) on e_W(CIV) --- alpha Spectral index (f({nu}) = {nu}**{alpha}) --- u_alpha Uncertainty flag on {alpha} --- previously-known high-z QSOs in SGP (II) RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec m(or) 'or' broad-band magnitude mag z redshift --- W(Ly1) rest-frame equivalent width (EW) of Lyman-{alpha}/NV blend 0.1nm W(CIV) rest-frame EW of CIV emission line 0.1nm alpha the spectral index derived from a power- law fit to the continuum --- REF reference (see paper) --- new UV excess quasars ID coordinate name --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec DATEy UT date of observation (year) a z redshift --- m(u) broad-band magnitude of 'u' mag m(bj) broad-band magnitude of 'bj' mag m(v) broad-band magnitude of 'v' mag m(or) broad-band magnitude of 'or' mag m(r) broad-band magnitude of 'r' mag l_m(i) limit flag of showing that m(i) is the upper limit --- m(i) broad-band magnitude of 'i' mag doc.tex ADC documentation file (LaTeX) (II) doc.txt ADC documentation file (II) Koichi Nakajima CDS 1994 Paul Kuin [ADC] 13-May-1997 Mar 03 UNKNOWN UNKNOWN 19-Jul-1993: Creation of catalogue VII/148 for Tables 1-4 of paper II. Copy from Hypathia, ADC, NASA. Modified to split Abs/Em W(CIV). 15-Jun-1993: Tables of paper I and II were received from H.Andernach, IAC, Tenerife, Spain. The catalogue was provided by courtesy of S.J. Warren to H. Andernach; it was numbered A129 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 17-Nov-1993: Creation of catalogues J/ApJS/76/1 and J/ApJS/76/23. 14-Mar-1994: Creation of catalogue VII/182, superseding above ones. (The date of the latest archiving, see the date of each file.) 13-May-1997: Updated Intro file to ReadMe standard. VII_182.xml The Cluster System of the Large Magellanic Cloud 7183 VII/183 Cluster System of the LMC The Cluster System of the Large Magellanic Cloud M Kontizas D H Morgan D Hatzidimitriou E Kontizas A&AS 84 527 1990 1990A&AS...84..527K Clusters, open Associations, stellar Magellanic Clouds A new catalogue of clusters in the Large Magellanic Cloud has been constructed from searches of the IIIa-J component of the ESO/SERC Southern Sky Atlas. The catalogue contains coordinate and diameter measurements of 1762 clusters in a 25 deg x 25 deg area of sky centered on the LMC, but excluding the very crowded 3.5 square deg region around the Bar. The distribution of these clusters appears as two superimposed elliptical systems. The higher density inner system extends over about 8 deg; the lower density outer system can be represented by 13 deg X 10 deg disc inclined at 42 deg to the line of sight. There are suggestions of two weak "arms" in the latter.
The Cluster System of the LMC Number Number of the cluster --- Name Name of the cluster (1) (2) number=3 (Table 3) Objects previously classified as clusters but excluded from catalog (Table 1). The numerical codes "c" are as follows: 1 Nothing detected 4 Association 2 Asterism or bright star 5 Nebula and/or dust cloud 3 Galaxy 6 Uncertain classification NGC objects No c No c No c No c No c --------------------------------------------------- 1557 1 1763 5 1929 5 1962 5 2035 5 1641 3 1769 5 1933 6 1965 5 2040 4 1669 3 1773 5 1934 5 1966 5 2069 4 1715 5 1820 4 1935 5 1970 5 2082 3 1737 6 1848 4 1936 5 2020 5 2103 5 1745 2 1892 3 1937 5 2029 5 2150 3 1747 4 1895 2 1945 5 2032 5 2187 3 1748 5 1925 4 1948 4 2034 4 2199 3 1760 4 IC objects No c No c No c No c No c --------------------------------------------------- 2105 5 2115 5 2126 5 2127 5 2128 5 2114 5 2116 5 SL objects No c No c No c No c No c --------------------------------------------------- 18 1 73 1 279 1 681 1 875 1 20 2 78 3 289 2 705 3 878 1 21 2 97 2 305 6 741 1 879 3 24 2 104 3 313 1 785 4 880 1 31 3 159 1 442 3 820 1 887 3 32 3 182 1 447 1 847 3 889 1 38 2 185 1 532 2 851 1 894 3 54 2 220 1 545 2 856 3 898 3 69 5 277 3 673 4 HS objects No c No c No c No c No c --------------------------------------------------- 1 3 17 3 53 1 163 1 312 6 2 3 18 3 54 3 170 6 339 6 3 2 19 3 55 2 171 3 344 1 4 3 20 3 57 2 176 2 364 2 5 3 21 3 69 3 183 3 392 3 6 3 22 2 71 3 204 3 394 3 7 3 24 1 79 2 209 2 418 6 9 3 25 3 89 3 222 2 423 5 10 1 29 2 123 3 244 4 449 3 11 3 34 2 126 1 246 1 451 3 12 1 42 2 145 2 271 2 452 3 14 2 45 3 146 3 276 2 454 3 15 2 47 3 150 3 278 3 455 3 16 2 49 6 160 2 297 6 LW objects No c No c No c No c No c --------------------------------------------------- 6 1 52 2 113 1 291 2 396 3 10 1 54 2 118 1 300 6 415 1 19 1 67 2 120 3 304 1 429 3 26 1 70 3 210 6 334 6 435 3 29 1 71 3 224 1 338 1 439 3 40 1 74 2 230 6 340 1 443 1 42 2 90 3 253 1 349 1 464 1 45 1 92 1 257 1 351 1 465 3 49 1 93 2 275 5 377 3 476 3 51 1 OH objects No c No c No c No c No c --------------------------------------------------- 5 6 13 2 20 6 24 6 28 3 7 6 18 6 23 6 26 6 32 6 --- RAh Right ascension B1950 (hours) h RAm Right ascension (minutes) min RAs Right ascension (seconds) s DE- Declination sign --- DEd Declination B1950 (degrees) deg DEm Declination (minutes) arcmin DEs Declination (seconds) arcsec Dist Distance in parsec pc Class C or L for each cluster according to whether it appeared compact or loose. --- Joseph Florsch CDS 1994 Mar 24 David Morgan (dhm@roe.ac.uk) VII_183.xml Survey of 108 E-S0 RSA galaxies 7184 VII/184 Survey of 108 E-S0 galaxies Survey of 108 E-S0 RSA galaxies R Michard J Marchal Astron. Astrophys. Suppl. Ser. 98 29 1993 1993A&AS...98...29M Survey of 108 E-S0 RSA galaxies R Michard J Marchal Astron. Astrophys. 283 779 1994 1994A&A...283..779M Survey of 108 E-S0 RSA galaxies R Michard J Marchal Astron. Astrophys. Suppl. Ser. 105 481 1994 1994A&AS..105..481M VII/51 : Revised Shapley-Ames Catalog of Bright Galaxies (Sandage+, 1981) Carter D., 1978, MNRAS 182, 797 de Vaucouleurs G. et al., 1976, Second Reference Catalogue of Bright Galaxies, Univ. Texas Publ. Michard R., Marchal J., 1994, A&A 283, 779 Michard R., Marchal J., 1994, A&AS 105 481 Michard R., Marchal J., 1993, A&AS 98, 29 Sandage A. & Tammann G., 1981, Revised Shapley-Ames Catalogue of Bright Galaxies, Cargenie Inst. of Washington (Cat. <VII/51>) Galaxies, Markarian Morphology Photometry Detailed data are available from our survey, results of which were published in A&A, in a series of papers. A survey has been performed of the morphological and photometric properties of 108 E-S0 galaxies out of a complete sample of 112: this sample is built from the Revised Shapley-Ames Catalogue (RSA) keeping objects with {delta}>-10deg and V_0_<3000km/s, rejecting SB0's and Local Group dwarfs. The data were mainly derived from our CCD observations at Observatoire de Haute-Provence: the camera allowed fields of 4x7arcmin (or 7x7 from the last run), the seeing being generally in the 2-3arcsec FWHM range. The measurements include the isophotal analysis according to Carter's (1978) principles, and the photometric profiles along the two main axis. Opposite semi-axis are measured separately to detect asymmetries.
Observed galaxies and characteristics of the frame with available data --- Prefix of name --- NGC NGC number --- Color Color of frame --- Code Code number of frame --- Type Hubble type from the Revised Shapley-Ames Catalogue (RSA) --- Inst. Instrumentation number=1 hpc 120 cm in Haute-Provence with CCD hpp id. with IIaO plates t2r 2 m at Pic du Midi, f/10 or f/8 reducer with CCD t2f id. , f/2.5 or f/3.5 reducer with CCD --- FWHM FWHM of Point Spread Function in arc sec arcsec SkyBr Sky brightness mag/arcsec2 Maj Major axis of external fully analysed isophote arcsec IsoBr Brightness of the same isophote, mag/arcsec2 Notes Individual notes number=2 (1) Frames from the Toulouse team, kindly provided by P. Poulain. (2) Photometric calibration from Michard and Simien, 1988. (3) Photometric calibration from Michard, 1985. (4) Galaxian center saturated. (5) Frames kindly obtained for us by P. Prugniel. (6) Frames kindly obtained for us by F. Simien. --- Main results of the morphological analysis of the studied galaxies. First list. (table2 of 1994A&AS..105..481M) NGC NGC Number --- RSA Revised Shapley-Ames Catalogue Hubble type --- T RC2 index (de Vaucouleurs Revised Morphological Type) --- Ph Photometric evidence for bulk-disk st = strong, ft = faint, cl = clear, no = not seen --- qmin Minimum axis ratio --- log(aq) Major axis of the isophote where qmin was taken [arcsec] e*4 Carter coefficient of e4 --- e*6 Carter coefficient of e6 measured at the same place as e*4 --- q25 Value of the axis ratio for the isophote mu=25 in V light --- DeltaPA Amplitude of the twist of the isophotes --- Bar Presence of a bar (bar or no) --- Dust Presence of dust duR = dust ring, duL = dust lane du- if of uncertain geometry, ??? if uncertainty, no = no detection --- Disk Nature of disk emDi = embedded disk, exDi = extended disk miDi = mixed disk, no = no detection ?Di if of dubful extension --- R/L Ring or lens presence rl- = inner ring, -oL = outer lens, roL = both seen, no = no detection --- Spi Spiral pattern presence spP = possible spiral pattern, no = no detection --- Env Envelope classification spH = spheroidal halo, thD = thick disk exD = extended disk, pec = peculiar envelope ? if not classified --- Asy Miscellaneous structure asyC = asymmetries with color effects asyG = asymmetries without color effects asy? = color class unknown no = no significant detected structure ? no suitable observations --- type Revised Hubble type, completed for E objects. diE = disky E, boE = boxyE, unE if of undeterminate subclass p added if the object has a peculiar envelope SAO, SAB0, SB0 as in the RC2, except that the r, s varieties are not noted --- Main results of the morphological analysis of the studied galaxies. Second list. (table3 of 1994A&AS..105..481M) NGC NGC number --- T RC2 index (de Vaucouleurs Revised Morphological Type) --- Type Revised and complete morphological classification of rsamorp --- VT Asymptotic magnitude either measured from our V frames, or sometimes converted form B frames through the RC2 B-V colors mag log(r*e) de Vaucouleurs radius [kpc] log(l*e) Corresponding semi-major axis [kpc] mu*e(V) Mean surface brightness of the effective isophote in V light mag/arcmin2 mu0 Adopted distance modulus mag BT0 Asymptotic magnitude converted to B light mag MT(B) Absolute magnitude mag log(R*e) Mean radius of the effective isophote [kpc] mu*e(B) Mean surface brightness of the effective isophote in B light mag/arcmin2 logD25 RC2-like parameter [0.1arcmin] logR25 RC2-like parameter --- Initial parameters for photometric measurements --- Prefix for NGC number --- NGC NGC number --- Color Color of the observation --- Frame Serial number for the frame --- OtherName Other name --- size pixel size arcsec FWHM FWHM of the PSF pix Nharm number of harmonics in Carter's isophotal representation (always 10) --- Niso number of isophotes in the table --- p1 Parameter used to describe the sky level number=1 Those parameters are in frame units and of "house keeping" interest --- p2 Parameter used to describe the sky level number=1 Those parameters are in frame units and of "house keeping" interest --- cal calibration constant mag pSuBr peak surface brightness of the galaxy mag SuBr surface brightness of the faintest measured isophote mag Average magnitudes on axis --- Prefix for NGC number --- NGC NGC number --- Color Color of the observation --- Frame Serial number for the frame --- a major axis of contour arcsec SuBra surface brightness corresponding to major axis of contour mag b minor axis of contour arcsec SuBrb surface brightness corresponding to minor axis of contour mag Differences between sectors --- Prefix for NGC number --- NGC NGC number --- Color Color of the observation --- Frame Serial number for the frame --- Dmaj Distance from center along major axis arcsec Dsubrmaj Difference of surface brightness at opposite major axis positions of the given central distance mag Dmin Distance from center along minor axis arcsec Dsubrmin Difference of surface brightness at opposite minor axis positions of the given central distance mag Gradients on the two axis --- Prefix for NGC number --- NGC NGC number --- Color Color of the observation --- Frame Serial number for the frame --- a major axis of contour arcsec GradSuBra Gradient of surface brightness along major axis mag/arcsec b minor axis of contour arcsec GradSuBrb Gradient of surface brightness along minor axis mag/arcsec Initial parameters for isophotal analysis --- Prefix for NGC number --- NGC NGC number --- Color Color of the observation --- Frame Serial number for the frame --- size Pixel size arcsec FWHM FWHM of the PSF pix Nharm Number of harmonics in Carter's isophotal representation (always 10) --- Niso Number of isophotes in the table --- p1 Parameter used to describe the sky level number=1 Those parameters are in frame units and of "house keeping" interest --- p2 Parameter used to describe the sky level number=1 Those parameters are in frame units and of "house keeping" interest --- p3 Parameter used to describe the sky level number=1 Those parameters are in frame units and of "house keeping" interest --- Cal Calibration constant mag Pint Peak intensity of the galaxy number=2 Those parameters are in frame units --- isof Level of faintest measures isophote number=2 Those parameters are in frame units --- PSuBr Peak surface brightness of the galaxy mag SuBrf Surface brightness of the faintest measured isophote mag Isophote parameters --- Prefix for NGC number --- NGC NGC number --- Color Color of the observation --- Frame Serial number for the frame --- Npix Number of pixels used to describe the isophote --- MaRE Major axis of the Reference Ellipse (RE) arcsec rRE Axis ratio of the RE 10-3 PArRE Position angle of the major axis of the RE deg C4 Coefficient of the 4th cosine harmonic 10-4 C6 Coefficient of the 6th cosine harmonic 10-4 C8 Coefficient of the 8th cosine harmonic 10-4 C10 Coefficient of the 10th cosine harmonic 10-4 C3 Coefficient of the 3rd cosine harmonic 10-4 S3 Coefficient of the 3rd sine harmonic 10-4 S2 Coefficient of the 2nd sine harmonic. This coefficient is expected to be zero if the isophote is reasonnably well defined. Significant values occur at low surface brightness and indicate a poor isophote representation. 10-4 S4 Coefficient of the 4th sine harmonic 10-4 S6 Coefficient of the 6th sine harmonic 10-4 SuBr Surface brightness of the isophote mag/arcsec2 Patricia Bauer CDS 1994 Sep 14 VII_184.xml IRAS 1.2 Jy Redshift Survey Data File 7185 VII/185 IRAS 1.2 Jy IRAS Redshift Survey IRAS 1.2 Jy Redshift Survey Data File M Strauss M Davis A Yahil J P Huchra Astrophys. J. 361 49 1990 1990ApJ...361...49S IRAS 1.2 Jy Redshift Survey Data File M Strauss J P Huchra M Davis A Yahil K B Fisher J Tonry Astrophys. J. Suppl. 83 29 1992 1992ApJS...83...29S IRAS 1.2 Jy Redshift Survey Data File K B Fisher J P Huchra M A Strauss M Davis A Yahil D Schlegel Astrophys. J. Suppl. 100 69 1995 1995ApJS..100...69F II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) II/174 : IRAS 2Jy Redshift Survey Data File (Strauss+ 1992) Infrared sources Photometry, infrared Redshifts This is an explanation of the redshift survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in a paper submitted for publication to the Astrophysical Journal Supplement. The survey contains 9897 objects selected from the IRAS database according to the criteria listed in that paper, briefly: F60 > 1.2 Jy; F60^2 > F12 f25; |b| > 5; high source density flag at 60 microns not raised. Thus, the file consists of both galaxies and Galaxian contaminants; this is explained below. The sample contains ~5320 galaxies, and 14 objects without id's at the present time.
The data file RAh Right Ascension B1950 (hours) The coordinates for all objects that appear in the IRAS PSC, Version 2, are from that source, and are given as B1950.0; there are also a few very large galaxies whose fluxes and coordinates are taken from the Large Optical Galaxy Catalog (Rice et al. 1988, ApJS, 68, 91). h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec nf12 log_10 of 12 um flux, in 0.1 Jy The IRAS fluxes are coded in a compact logarithmic form: The 12 micron flux is related to the integer nF12 by F12 = 10.^(nF12/1000 - 1.); similarly for the other fluxes. The fluxes are taken from the PSC, unless: 1. The object is extended at 60 microns (see extendflag below); 2. The object is variable (see varflag below); 3. The object is of moderate flux quality at 60 microns (see Fq60 below). In these cases, we have obtained one-dimensional addscan's of the data and used the zero-crossing flux from the median scan's in all four bands, as supplied by SCANPI. Those sources flagged as extended in Rice et al. have fluxes from that source. [0.1Jy] nf25 log_10 of 25 um flux, in 0.1 Jy [0.1Jy] nf60 log_10 of 60 um flux, in 0.1 Jy [0.1Jy] nf100 log_10 of 100 um flux, in 0.1 Jy [0.1Jy] IDtype IRAS PSC identification The idtype is taken directly from the PSC; Idtype ranges from 1 to 4 and states whether an association was found is an extragalactic catalog (1), stellar catalogs (2), other catalogs (3), or matches in multiple types of catalogs (4). --- ExtendFlag IRAS PSC flag for extended objects The extendflag indicates whether or not an object is flagged as extended (SES(2) flag) in the psc. extendflag = 0 Not extended 1 Extended at 12 microns 2 Extended at 25 microns 3 Extended at 12 and 25 microns 4 Extended at 60 microns 5 Extended at 12 and 60 microns 6 Extended at 25 and 60 microns 7 Extended at 12, 25, and 60 microns 8 Extended in Rice et al --- CC IRAS PSC cirrus flag The correlation coefficient is taken from the PSC and represents the best correlation coefficient between a hours-confirmed scan and the point source template at 60 microns in the Point Source Data Base; see the Explanatory Supplement for details. A means 99% or better correlation, B is between 98 and 99% and so on. --- VarFlag IRAS PSC variability flag The varflag is a measure of variability in 12 and 25 microns. n No measure of variability available. 0 No variability measured. N Variability between 1 and 10%. 1 Variability between 10 and 20% and so on. --- StatusFlag Object identification flag The statusflag indicates the identification of the source, and, if it is a galaxy, the source of the redshift: Galaxies: O,H,Z,F,B,D. The distinction between these is uninteresting, although Z indicates a source drawn from John Huchra's private version of ZCAT. L: Local Group galaxy. This is given a separate flag. Non-galaxies: M: HII region in external galaxy. S: Star s: Emission line star C: Cirrus or dark cloud P: Planetary nebula R: Reflection Nebula ? or E: Unidentified field. These labels are by no means complete; we observed only a fraction of these sources at the telescope. See Strauss et al. 1990 and Yahil et al. 1991 (ApJ, 372, 380) for a discussion of our estimate of the number of sources flagged as cirrus that are indeed galaxies. --- fq12 IRAS PSC Flux qual. flag 12um The flux qualities are taken from the PSC; one number between one and three is given for each band: 1: Not detected 2: Moderate flux quality 3: Good flux quality If the flux given is from the PSC (as opposed to ADDSCAN), the flux listed in a band with flux quality 1 will be an upper limit. --- fq25 IRAS PSC Flux qual. flag 25um --- fq60 IRAS PSC Flux qual. flag 60um --- fq100 IRAS PSC Flux qual. flag 100um --- optID Optical counterpart to the object Optical identification is from a matching of the combined UGC, Zwicky, and NGC catalogs. --- mag Optical magnitude, where available Magnitudes are from the same source, and are not complete. mag Hvel Heliocentric velocity Redshifts and errors are either as quoted in the literature, or measured by us. All are heliocentric. km/s e_Hvel Heliocentric velocity error km/s r_Hvel Code for source of redshift Source is a four-digit number that codes the redshift source from ZCAT. --- Ttype de Vaucouleurs' T-type Ttype is the type of the galaxy from ZCAT. --- UGC/ESO object ID from UGC or ESO catalog first 5 bytes is number last byte is letter or blank Unumber is either the UGC or ESO number of the source. --- Spectrum Internal flag coding the optical spect Spectrum is an internal index for the optical spectrum, if one exists, of the galaxy in the CfA database. --- comments Miscellaneous comments Comments are taken from ZCAT. --- pf12 log_10 of 12 um flux, in 0.1 Jy Fluxes of the source as listed in the IRAS Point Source Catalog for those sources with ADDSCAN fluxes in columns 17-32; they are coded the same way as the earlier fluxes are. [0.1Jy] pf25 log_10 of 25 um flux, in 0.1 Jy [0.1Jy] pf60 log_10 of 60 um flux, in 0.1 Jy [0.1Jy] pf100 log_10 of 100 um flux, in 0.1 Jy [0.1Jy] Michael Strauss IAS 1995 Feb 06 People may contact Michael Strauss at strauss@astro.princeton.edu if they have questions about these files. UNKNOWN UNKNOWN * MCG and PK numbers which were truncated in the original catalogue file have been replaced at CDS (Francois Ochsenbein, 10-Oct-1997) UNKNOWN UNKNOWN There is a supplementary file, exclude.lis which contains the number of the lune bins that are excluded (see Paper 1 for a full description). There is a series of Fortran programs in exclude.f that should be used to decide if a given object is in the excluded regions or not. First, run the program write_lmask, which reads the exclude.lis file and creates a binary file lmask.lis, which has much faster I/O. This only need be done once. Your code will need to call init_lmask to read in lmask.lis, and thereafter zones or not. VII_185.xml Catalogue of Galaxies in Abell 3744 7186 VII/186 Catalogue of Galaxies in A3744 Catalogue of Galaxies in Abell 3744 R A Cameron PhD Thesis, Sydney ??? ??? 1988 Clusters, galaxy Radial velocities This catalogue contains the positions and radial velocities of 47 galaxies.
Positions and radial velocities Name Galaxy running number --- m_Name Multiplicity index on galaxy running number --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec RVabs Heliocentric cz velocities measured from the cross-correlation between absorption features in the galaxy and template spectra km/s e_RVabs rms uncertainty associated with the absorption velocities km/s R Tonry and Davis R factors for the cross-correlations --- RVem Heliocentric cz velocities obtained from emission lines redshifts km/s o_RVem Number of emission lines measurements for the galaxy --- e_RVem rms uncertainty on emission velocity measures for those galaxies with more than one emission ine velocity km/s Patricia Bauer CDS 1995 Mar 01 Cameron R.A. <cameron@ossek.nrl.navy.mil> VII_186.xml Zwicky Galaxy Catalog 7190 VII/190 Zwicky Galaxy Catalog Zwicky Galaxy Catalog F Zwicky E Herzog P Wild Vol. I Pasadena: California Institute of Technology ??? ??? 1960 1960 Zwicky Galaxy Catalog F Zwicky E Herzog Vol. II Pasadena: California Institute of Technology ??? ??? 1963 1963 Zwicky Galaxy Catalog F Zwicky E Herzog Vol. III Pasadena: California Institute of Technology ??? ??? 1966 1966 Zwicky Galaxy Catalog F Zwicky E Herzog Vol. IV Pasadena: California Institute of Technology ??? ??? 1968 1968 Zwicky Galaxy Catalog F Zwicky M Karpowicz C T Kowal Vol. V Pasadena: California Institute of Technology ??? ??? 1965 1965 Zwicky Galaxy Catalog F Zwicky C T Kowal Vol. VI Pasadena: California Institute of Technology ??? ??? 1968 1968 Zwicky Galaxy Catalog M Kalinkov I Valtchanov I Kuneva Institute of Astronomy, Bulgarian Academy of Sciences ??? ??? 1996 1996 Galaxy catalogs This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley & Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zg_ori.dat and zg_add.dat. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.
The original information from CGCG for galaxies. ZG Zwicky galaxy number. Sequential number of Zwicky galaxies sorted by RA. We have followed the appropriate convention - for objects with the same RA the Dec is ascending (note that the distributed ADC catalog (ADC #7049 or CDS VII/49) does not correspond to the original ordering of objects in the fields F2 to F23 and F25). The coordinates of galaxies in the Coma cluster center are given with usual accuracy as for other galaxies. --- RAh Right ascension 1950 (hours). h RAm Right ascension 1950 (minutes). min DE- Declination 1950 (sign). --- DEd Declination 1950 (degrees). deg DEm Declination 1950 (minutes). arcmin Pmag Zwicky magnitude. mag Name Name (N=NGC, I=IC). If the column width for Name is not sufficient, then a sign '+' is put and the continuation is in the Notes column. --- add Entry in zwi_gal.add. --- Notes Notes. In principle all Zwicky descriptions are kept but several abbreviations are used: c - compact p - peculiar dneb - double nebula qneb - quadruple nebula dsys - double system qsys - quadruple system g(s) - galaxy(-ies) S(s) - spiral(s) I - irregular sys - system msys - multiple system tsys - triple system --- Field1 First field where the galaxy may be found and consequent number. The polar fields are 370A and 370B. The additional regions for fields 196 and 298 are denoted as 196A and 298A. Most of galaxies in these fields are contained in other fields too. The appropriate designation of galaxies in the CGCG is according to the Field number and consequent number of the galaxy in this field. Generally, it is fulfilled for all fields with following exceptions: There are four galaxies inserted, with the same number as the previous ones but with suffix 'E' not to change the ordering in the published CGCG: F39-130E (ZG 12383=1118.6+0328), between F39-130 and 131, F41-53E (ZG 14486=1212.7+0602), F70-135E (ZG 15206=1228.0+1246), F126-8E (ZG 12073=1110.8+2226). We follow the wrong ordering for objects F42-72, 73, 74 (misprint in RA for object F42-72), as well as for F42-79, 80 (misprint in RA of F42-79) and F385-127, 128 (wrong original ordering). (Declinations of objects ZG 7786 (F264-34/NGC 2694) and ZG 7787 (F264-35/NGC 2693) are misprinted in the CGCG (as well as in the ADC version), but it does not change the ordering). --- Field2 Second field ...(if any). --- Field3 Third field ...(if any). --- Data from other catalogs given in CGCG. ZG Zwicky galaxy number. --- m_ZG Multiplicity suffix Note that zg_add.dat contains some objects with the same Zwicky number with A and B. These are ZG 447A, ZG 2180A and B, ZG 6227A, Z8448A and B, ZG 20607A which are components according to other authors. Notes on tP: The type for ZG 16032 according to the catalog of Pettit (1954) is longer and there is a sign '+' which means that the type continues in Notes of the file zg_ori.dat. Notes on tHMS: The type for ZG 20230 according to Humason et al. (1956) is longer and there is a sign '+' which means that the type continues in Notes of the file zg_ori.dat. --- Name Name (N=NGC, I=IC). --- mSA Magnitude from Shapley & Ames (1932). mag tSA Type from Shapley & Ames (1932). --- mB Magnitude from Bigay (1951). mag tB Type from Bigay (1951). --- mP Magnitude from Pettit (1954). mag tP Type from Pettit (1954). --- mHMS Magnitude from Humason et al. (1956). mag tHMS Type from Humason et al. (1956). --- mH Magnitude from Holmberg (1958). mag tH Type from Holmberg (1958). --- Vel Velocity. km/s CDS Catalogues Service CDS 1996 Mar 06 We are very indebted to H.C. Corwin, A. and G. de Vaucouleurs, J.P. Huchra, G. Paturel and F. Ochsenbein for discussions and supply of information. M.K. and I.K. are deeply grateful to H. van der Laan, Director General of ESO, A. Omont, Director of Institute d'Astrophysique, Paris and R. Williams, Director of the Space Telescope Science Institute for the opportunity to work in the corresponding institutes. The compilation of the catalog is partly supported by the National Research Fund of the Bulgarian Ministry of Education, Science and Technology (contract F469/1994). VII_190.xml A catalogue of southern dark clouds 7191 VII/191 Catalogue of Southern Dark Clouds A catalogue of southern dark clouds M Hartley R N Manchester R M Smith S B Tritton W M Goss Astron. Astrophys. Suppl. Ser. 63 27 1986 1986A&AS...63...27H VII/7 : Lynds' Catalogue of Dark Nebulae (LDN) Nebulae dark clouds interstellar matter star formation Gould's Belt A catalogue of 1101 dark clouds has been compiled from visual inspection of ESO/SERC Southern J survey plates for declinations south of -33deg. This catalogue complements that of Lynds (1962ApJS....7....1L) which is based on the Palomar Sky Survey. Equatorial positions of accuracy 10 arcsec or better are listed for each cloud along with size (major axis x minor axis), density class and ESO/SERC field number. Galactic coordinates, derived from the equatorial positions, are used to define a name for each cloud. Complexes, consisting of several separately identifiable concentrations, are listed and identified by a trailing C on the name. The conclusions of Lynds, that clouds are concentrated along the galactic equator and toward the galactic centre, are reinforced. No clear connection with Gould's Belt is evident in the distribution of southern clouds.
The catalogue of Southern Dark Clouds (DCld) DCld Dark Cloud name The name is made from galactic longitude and latitude of the centroid. --- n_DCld 'C' indicates a complex structure --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Size1 Largest angular size In the case of some curved and elongated clouds, Size1 represents the total length of the cloud rather than the overall dimension; therefore the product of Size1 x Size2 approximates the area of the cloud. arcmin --- separator --- Size2 Second angular size arcmin Density Density class densities are represented by a 3-letter scale with A being the most dense and C the least dense. Statistics and comparison with Lynds (1962ApJS....7....1L) opacity classes: ------------------------------------------------------------ Density No. of Mean Size Median Size Lynds' Class Clouds (sq. arc min.) (sq. arc min.) opacity ------------------------------------------------------------ A 432 100 22 6 B 493 560 65 4 or 5 C 176 420 105 <= 3 ------------------------------------------------------------ All 1101 355 50 --- Field Field or Plate number of ESO/SERC survey --- Comments Text of Comments the following abbreviations are used: CG = cometary globule DC = dark cloud RN = reflection nebula S-O = Sco-Oph complex which extends into the Sct region. Designations preceded by S refer to Sandqvist and Lindroos (1976A&A....53..179S) and Sandqvist (1977A&A....57..467S) --- James Marcout, Francois Ochsenbein CDS 1996 Feb 21 UNKNOWN UNKNOWN The catalogue was keypunched at CDS. UNKNOWN UNKNOWN Sources from this catalogue are preferably designated <<DCld LLL.l+BB.b>> rather than <<DC LLL.l+BB.b>> VII_191.xml Contemporary Index Into Halton Arp's Peculiar Galaxies 7192 VII/192 Arp's Peculiar Galaxies Contemporary Index Into Halton Arp's Peculiar Galaxies D Webb SKY & Telescope 92-1 92 1996 1996S&T....92...92W Galaxy catalogs Historical catalog Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.
The galaxies identified in Arp's Atlas of Peculiar Galaxies represent a remarkable cross-section of observing opportunities. With the wide availability of inexpensive CCD cameras and increasing aperture of inexpensive commercial telescopes, more of the Arp list is accessible to more observers. Many of the objects so catalogued were anonymous galaxies in 1966 and have subsequently been characterized and named. The NASA-IPAC Extragalactic Database (NED) provided most correlations and other sources identified others. Please refer to http://users.aol.com/arpgalaxy for further information.
list of Arp views with imaging data Arp_no Arp number from original catalog number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. --- Name Common name (group or brightest) The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. --- Rah Right Ascension 2000 (hours) number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. h RAm Right Ascension 2000 (minutes) number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. min DE- Declination 2000 (sign) number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. --- DEd Declination 2000 (degrees) number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. deg DEm Declination 2000 (minutes) number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. arcmin Size Long dimension of Arp's original photo Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. arcmin Orient Orientation of Arp photo Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= The Name is the most common name of the brightest galaxy in the view or the common name of the group of interacting galaxies. Where the view is a main galaxy with companion, both names are indicated with the companion in abbreviated form. The Right Ascension and Declination is of the brightest galaxy and not the center of Arp's original photo. number= Size is the longest dimension of the rectangular field of view of the image published in Arp's 1966 Atlas. This information is provided to assist the observer in framing the view for imaging. number= Orientation is the alignment of the top (narrow side) of Arp's original photo. For example, "E" means the published photo is a rectangle with the long side running east to west with east at the top. number= This table identifies all named galaxies involved in Arp's Atlas of Peculiar Galaxies. It is provided in Right Ascension sequence with all of the galaxies in a given Arp view together. Occasionally a galaxy from one Arp view will intervene between galaxies of another Arp view, due to both Arp's location at the same Right Ascension. Observational attributes for each such galaxy are provided as well. --- fl_245 Focal length for CB245 CCD Camera number=1 These three columns are the focal lengths in inches of the optical system necessary to duplicate Arp's original image using the named CCD camera. 2.54cm fl_ST6 Focal length for SBIG ST6 CCD Camera number=1 These three columns are the focal lengths in inches of the optical system necessary to duplicate Arp's original image using the named CCD camera. 2.54cm fl_ST5 Focal length for SBIG ST5 CCD Camera number=1 These three columns are the focal lengths in inches of the optical system necessary to duplicate Arp's original image using the named CCD camera. 2.54cm list and info for involved galaxies Arp_no Arp number from original catalog number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. --- Name Common name of galaxy number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. --- VT Total V-magnitude Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. mag u_VT Uncertain magnitude = ? number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. --- size_g Dimensions of galaxy number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. --- u_size_g Uncertain size = ? number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. --- MType Morphological Type Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. --- Uchart Uranometria chart number Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. --- RAh Right Ascension 2000 (hours) number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. h RAm Right Ascension 2000 (minutes) number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. min RAs Right Ascension 2000 (seconds) number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. s DE- Declination 2000 (sign) number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. --- DEd Declination 2000 (degrees) number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. deg DEm Declination 2000 (minutes) number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. arcmin DEs Declination 2000 (seconds) number= Magnitude sources and types vary. In general, where the galaxy appears in Uranometria, the Deep Sky Field Guide's algorithm for computing VT is assumed. Where the galaxy is not so listed, a variety of magnitudes are used but not distinguished or recorded. Sources include predominantly RC3 and PGC. number= Where available, the long form mixed case Hubble morphological type (SB(rs)bc) is provided. In some cases the simplified all caps form (IBS9P) is used. Where no such designation was available, some sources provide a phrase like "disturbed", "DBL SYS" or "Multiple Sys". number= Galaxies listed in the Uranometria 2000.0 Deep Sky Field Guide are indicated by reference to the chart number. Those galaxies so listed which do not appear on the chart are field galaxies listed in the Field Guide's notes column. arcsec Dennis Webb Johnson Space Center Astro. Society 1996 Jul 19 This Research Made Use Of The Nasa/Ipac Extragalactic Database (Ned) Which Is Operated By The Jet Propulsion Laboratory, Caltech, Under Contract With The National Aeronautics And Space Administration Al Kelly computed image sizes and required focal lengths for contemporary CCD cameras. He also photographed a few to verify that amateur CCD cameras can see faint peculiarity. Mike Brown loaded galaxy size information and audited the list against the MegaStar Deep Sky Atlas database (RC3 and PGC) Emil Bonanno precessed coordinates from epochs 1950 to 2000. Barbara Wilson provided desire, consultation and encouragement. Lara Lenoir audited the list against the Deep Sky Field Guide, and MegaStar (RC3 and PGC). Halton C. Arp for not being offended at the interest in his early work. VII_192.xml Mark III Catalog of Galaxy Peculiar Velocities: Distances for Groups and Single Galaxies Homogeneous Velocity-Distance Data for Peculiar Velocity Analysis. I. Calibration of Cluster Samples 7198 VII/198 Mark III Catalog of Galaxy Peculiar Velocities Mark III Catalog of Galaxy Peculiar Velocities: Distances for Groups and Single Galaxies Homogeneous Velocity-Distance Data for Peculiar Velocity Analysis. I. Calibration of Cluster Samples J A Willick S Courteau S M Faber D Burstein A Dekel T Kolatt Astrophys. J. 446 12 1995 1995ApJ...446...12W Mark III Catalog of Galaxy Peculiar Velocities: Distances for Groups and Single Galaxies Homogeneous Velocity-Distance Data for Peculiar Velocity Analysis. I. Calibration of Cluster Samples J A Willick S Courteau S M Faber D Burstein A Dekel T Kolatt Astrophys. J. 457 460 1996 1996ApJ...457..460W Mark III Catalog of Galaxy Peculiar Velocities: Distances for Groups and Single Galaxies Homogeneous Velocity-Distance Data for Peculiar Velocity Analysis. I. Calibration of Cluster Samples J A Willick S Courteau S M Faber D Burstein A Dekel M A Strauss Astrophys. J. Suppl. 109 333 1997 1997ApJS..109..333W Radial velocities Galaxy catalogs galaxies: distances and redshifts galaxies: peculiar Tully-Fisher and Dn-sigma distances, radial velocities, and associated catalog and observational data for the spiral, irregular, and elliptical galaxies that comprise the Mark 3 catalog are given in 5 different kinds of tables for seven separate data sets. Users interested only in the resulting distances need use only the files listed in sections 3 (Grouped spiral distance files), 4 (Elliptical galaxy distance files), and 5 (Comparison of galaxy distances).
The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match ************** IMPORTANT NOTE/DISCLAIMER In all cases, the Basic data files try to give the data as either published or otherwise given to us by the original author(s). In contrast, the Spiral Galaxy distance files contain data as homogenized by the authors' methodology. In many cases, value of radial velocity may differ by up to 50 km/sec (in the case of Local Group velocities), owing to both round-off errors in our computer programs and to differences in how to transform from one velocity reference frame to another. Similar, values of eta may differ in the last decimal place by up to 0.004. Only if much larger differences are found do the originators of these files wish the user to contact them. As errors are inevitable in a compendium of this size, notice of large errors found is much appreciated.
Mark 3 AHM field data_1 file RC3num Number in computer-readable RC3 file number=1 RC3num, RC2num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following four catalogs, as stored in Ultrix format by Burstein. RC2num and UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC2 catalog also has Holmberg (1958) stored for galaxies in common. A zero for any record number indicates galaxy not in that catalog. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) RC2num - RC2 (de Vaucouleurs et al. 1976); original version from Ohio State, pre-1980. UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. Likewise, Catnum is a record number uniquely assigned to each Aaronson et al. galaxy in the Tormen and Burstein (1995, ApJS 96, 123) analysis. --- RC2num Number in computer-readable RC2 file number=1 RC3num, RC2num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following four catalogs, as stored in Ultrix format by Burstein. RC2num and UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC2 catalog also has Holmberg (1958) stored for galaxies in common. A zero for any record number indicates galaxy not in that catalog. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) RC2num - RC2 (de Vaucouleurs et al. 1976); original version from Ohio State, pre-1980. UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. Likewise, Catnum is a record number uniquely assigned to each Aaronson et al. galaxy in the Tormen and Burstein (1995, ApJS 96, 123) analysis. --- UGCnum Number in computer-readable UGC file number=1 RC3num, RC2num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following four catalogs, as stored in Ultrix format by Burstein. RC2num and UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC2 catalog also has Holmberg (1958) stored for galaxies in common. A zero for any record number indicates galaxy not in that catalog. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) RC2num - RC2 (de Vaucouleurs et al. 1976); original version from Ohio State, pre-1980. UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. Likewise, Catnum is a record number uniquely assigned to each Aaronson et al. galaxy in the Tormen and Burstein (1995, ApJS 96, 123) analysis. --- ESOnum Number in computer-readable ESO file number=1 RC3num, RC2num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following four catalogs, as stored in Ultrix format by Burstein. RC2num and UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC2 catalog also has Holmberg (1958) stored for galaxies in common. A zero for any record number indicates galaxy not in that catalog. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) RC2num - RC2 (de Vaucouleurs et al. 1976); original version from Ohio State, pre-1980. UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. Likewise, Catnum is a record number uniquely assigned to each Aaronson et al. galaxy in the Tormen and Burstein (1995, ApJS 96, 123) analysis. --- Catnum Unique number in Mark 3 AHM catalog number=1 RC3num, RC2num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following four catalogs, as stored in Ultrix format by Burstein. RC2num and UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC2 catalog also has Holmberg (1958) stored for galaxies in common. A zero for any record number indicates galaxy not in that catalog. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) RC2num - RC2 (de Vaucouleurs et al. 1976); original version from Ohio State, pre-1980. UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. Likewise, Catnum is a record number uniquely assigned to each Aaronson et al. galaxy in the Tormen and Burstein (1995, ApJS 96, 123) analysis. --- Gp_code Group number code number=2 Galaxies were assigned to groups/clusters by original Aaronson et al. papers. [Note that these groups do not correspond to the Mark III groups formed as described by Willick et al. 1996.] Each group/cluster is assigned a numerical code in this table. The codes are: -1: NOT CLASSIFIED 60: N5566 GROUP 0: NOT ASSIGNED 61: GRUS 1: PISCES 62: N24/45 2: A 400 63: N134 3: A 539 64: N701/755 4: CANCER 65: N2336 5: A1367 66: N2841 6: COMA 67: N3079/U5459 7: Z74-23 68: N3184 8: HERCULES 69: N3521 9: PEGASUS 70: LEO TRIPLET 10: A2634/66 71: Can Van I 12: HYDRA 72: N5033 13: N3557 73: M51 14: CEN30 74: N5371 15: CEN45 75: N5364 16: ANTLIA 76: N5676 17: ESO508 77: N5866 18: PAVO 78: N6070 51: LOCAL CALIBRATORS 79: N7320/7331 52: VIRGO, MAIN CLUSTER 80: N7537/7541 53: N1023 54: ERIDANUS 55: FORNAX 56: LEO 57: URSA MAJOR 58: COMA I 59: VIRGO, SOUTH See note (1) for a82file1.dat --- A-ext_1 4(E(B-V))_1, Burstein-Heiles method number=3 Two values of Burstein-Heiles E(B-V) are given for completeness. The value labeled _1 is for the present data. The value labeled _2 is what was used in the Mark II Catalog of Peculiar Velocities, as electronically distributed by Burstein starting in 1989. Differences of 0.02 to 0.06 in 4(E(B-V)) are evident, owing to issues explained in Burstein and Heiles (1984, ApJS 54, 33). mag A-ext_2 4(E(B-V))_2, BH method, but from Mark II number=3 Two values of Burstein-Heiles E(B-V) are given for completeness. The value labeled _1 is for the present data. The value labeled _2 is what was used in the Mark II Catalog of Peculiar Velocities, as electronically distributed by Burstein starting in 1989. Differences of 0.02 to 0.06 in 4(E(B-V)) are evident, owing to issues explained in Burstein and Heiles (1984, ApJS 54, 33). mag Log_D_g Log D_g, units of 0.1 arcmin number=4 D_g is the fiducial diameter used in this analysis, based on the inclination-corrected diameter taken from the RC3 but making the following correction: log D_g = log D_25(RC3) - log(1-EXT/3.35), for Galactic extinction effects on diameter. It is important to note that Log D_g is in RC3 units of 0.1 arcmin. The Aaronson published value of log D_1 is given as Log_D_1 (bytes 52-55), 0.1 arcmin units. 9.99 is given if no value available. .1arcmin Log_D_1 Aaronson publ Log D_1, 0.1 arcmin number=4 D_g is the fiducial diameter used in this analysis, based on the inclination-corrected diameter taken from the RC3 but making the following correction: log D_g = log D_25(RC3) - log(1-EXT/3.35), for Galactic extinction effects on diameter. It is important to note that Log D_g is in RC3 units of 0.1 arcmin. The Aaronson published value of log D_1 is given as Log_D_1 (bytes 52-55), 0.1 arcmin units. 9.99 is given if no value available. .1arcmin Log_a/b1 Log (axial ratio) RC3 or ESO number=5 Log_a/b1 is the log of the axial ratio as taken from the RC3 or, if not available there, taken from the original ESO data if an ESO galaxy. In the case where no independent axial ratio is in a catalog, an axial ratio was derived from the given Aaronson et al. inclination by inverting their formula. Log_a/b2 is the log of the axial ratio taken from Aaronson et al. --- Log_a/b2 Log (axial ratio) Aaronson original number=5 Log_a/b1 is the log of the axial ratio as taken from the RC3 or, if not available there, taken from the original ESO data if an ESO galaxy. In the case where no independent axial ratio is in a catalog, an axial ratio was derived from the given Aaronson et al. inclination by inverting their formula. Log_a/b2 is the log of the axial ratio taken from Aaronson et al. --- Inclin1 Inclination, RC3, no 3 deg corr number=6 Inclin1 is the inclination of galaxy as given by RC3 axial ratio and the Aaronson et al. formulation (i.e., assuming q = 0.2), but without assuming a 3 deg correction to inclinat as applied by Aaronson et al. in their papers. Inclin2 is the inclination listed in the Aaronson et al. papers. Inclin3 is Inclin1 with 3 deg added to be in accord with Aaronson et al. formulation. InclinH comes from Han (1992) Ph. D. thesis on cluster galaxies. This value is null (0) for the field data set. deg Inclin2 Inclination, RC3, with 3 deg corr number=6 Inclin1 is the inclination of galaxy as given by RC3 axial ratio and the Aaronson et al. formulation (i.e., assuming q = 0.2), but without assuming a 3 deg correction to inclinat as applied by Aaronson et al. in their papers. Inclin2 is the inclination listed in the Aaronson et al. papers. Inclin3 is Inclin1 with 3 deg added to be in accord with Aaronson et al. formulation. InclinH comes from Han (1992) Ph. D. thesis on cluster galaxies. This value is null (0) for the field data set. deg Inclin3 Inclination, original Aaronson number=6 Inclin1 is the inclination of galaxy as given by RC3 axial ratio and the Aaronson et al. formulation (i.e., assuming q = 0.2), but without assuming a 3 deg correction to inclinat as applied by Aaronson et al. in their papers. Inclin2 is the inclination listed in the Aaronson et al. papers. Inclin3 is Inclin1 with 3 deg added to be in accord with Aaronson et al. formulation. InclinH comes from Han (1992) Ph. D. thesis on cluster galaxies. This value is null (0) for the field data set. deg InclinH Han (1992) inclination number=6 Inclin1 is the inclination of galaxy as given by RC3 axial ratio and the Aaronson et al. formulation (i.e., assuming q = 0.2), but without assuming a 3 deg correction to inclinat as applied by Aaronson et al. in their papers. Inclin2 is the inclination listed in the Aaronson et al. papers. Inclin3 is Inclin1 with 3 deg added to be in accord with Aaronson et al. formulation. InclinH comes from Han (1992) Ph. D. thesis on cluster galaxies. This value is null (0) for the field data set. deg GLON Galactic longitude deg GLAT Galactic latitude deg Name Galaxy Name number=7 N = NGC (first name preference) I = IC (2nd preference) U = UGC (Nilson 1973) (3rd preference) E = ESO (Lauberts 1982) (3rd preference) Z = Zwicky, field+number (4th preference) A = Anonymous, RA (hr,min), Dec (deg) (4th preference) --- RC3_type RC3 galaxy type code --- RC2typn Numerical Code for RC2 galaxy types number=8 RC2 galaxy types are given numerical codes in the RC2. The code used here slightly revises that code, giving 0 for true S0/a galaxies, and -7 for IO galaxies. Photometric Galaxy Type is the galaxy type assigned each galaxy based on the growth curve analysis of Tormen and Burstein. 1 = S0, Sa and Sab 2 = Sb and Sbc 3 = Sc and Scd 4 = Sd to Im --- Phot_typ Photometric galaxy type, Tormen-Burstein number=8 RC2 galaxy types are given numerical codes in the RC2. The code used here slightly revises that code, giving 0 for true S0/a galaxies, and -7 for IO galaxies. Photometric Galaxy Type is the galaxy type assigned each galaxy based on the growth curve analysis of Tormen and Burstein. 1 = S0, Sa and Sab 2 = Sb and Sbc 3 = Sc and Scd 4 = Sd to Im --- Mark 3 AHM field data_2 file RC3num Number in computer-readable RC3 file number=1 See note (1) for a82file1.dat. --- RC2num Number in computer-readable RC2 file number=1 See note (1) for a82file1.dat. --- UGCnum Number in computer-readable UGC file number=1 See note (1) for a82file1.dat. --- ESOnum Number in computer-readable ESO file number=1 See note (1) for a82file1.dat. --- Catnum Unique number in Mark 3 AHM catalog number=1 See note (1) for a82file1.dat. --- Gp_code Group number code number=2 See note (2) for a82file1.dat. --- GLON Galactic longitude deg GLAT Galactic latitude deg q_Hmag_g Quality parameter for H_g number=3 Quality parameter for H_g: 1 = likely error less than 0.2 mag 2 = likely error 0.2 - 0.35 mag 3 = likely error in excess of 0.35 mag --- Hmag_g H_g at the log (D/D_g) = -0.5 diameter number=4 H_g, the H magnitude at the log (D/D_g) = -0.5 diameter (see note (4) for a82file1 for definition of D_g) corrected only for Galactic extinction. The inclination correction dependence of H_g is determined in a separate paper by Willick et al. (1996). The corresponding published H-0.5 mag of Aaronson et al. is given as HmagAHM (bytes 59-64). mag HmagAHM Aaronson et al publ galaxy H mag number=4 H_g, the H magnitude at the log (D/D_g) = -0.5 diameter (see note (4) for a82file1 for definition of D_g) corrected only for Galactic extinction. The inclination correction dependence of H_g is determined in a separate paper by Willick et al. (1996). The corresponding published H-0.5 mag of Aaronson et al. is given as HmagAHM (bytes 59-64). mag diffHmag Hmag_g minus HmagAHM mag HelioV Heliocentric radial velocity number=5 Heliocentric radial velocity taken primarily from original Aaronson et al. paper. For 23 galaxies, HelioV taken from NASA Extragalactic Database as of mid-1994. See Tormen and Burstein for details. km/s DelV "Raw" HI rotation velocity width number=6 "Raw" HI rotation velocity width, km/sec. This is the value as would be observed without any inclination correction. See Tormen and Burstein for details. km/s Lg_DelVA Aaronson publ log (Corr HI vel width) number=7 Lg_DelVA is the original log (HI profile velocity width) as published by Aaronson et al. Note that this does not, in general, correspond to the value of eta in the file a82_s, because galaxy inclinations were recomputed for the Mark III catalog. See Willick et al. 1997. --- HI_flux Aaronson publ HI flux number=8 The HI flux in the profile, expressed in units of Jy*km/s. The AHM papers typically quote an error of around 0.002 - 0.0025 Jy, which needs to be multiplied by the observed width to get an error for the flux. Given a typical width of 400 km/s, this translates to an observational error of 0.8 - 1 Jy*km/s. Jy*km/s Name Galaxy Name number=9 N = NGC (first name preference) I = IC (2nd preference) U = UGC (Nilson 1973) (3rd preference) E = ESO (Lauberts 1982) (3rd preference) Z = Zwicky, field+number (4th preference) A = Anonymous, RA (hr,min), Dec (deg) (4th preference) --- RC3_type RC3 galaxy type code --- Mark 3 AHM field data_3 file PGCnum Principal Galaxy Catalog number --- RC3num Number in computer-readable RC3 file number=1 See note (1) for a82file1.dat --- RC2num Number in computer-readable RC2 file number=1 See note (1) for a82file1.dat --- UGCnum Number in computer-readable UGC file number=1 See note (1) for a82file1.dat --- ESOnum Number in computer-readable ESO file number=1 See note (1) for a82file1.dat --- Catnum Unique number in Mark 3 AHM catalog number=1 See note (1) for a82file1.dat --- Gp_code Group number code number=2 See note (2) for a82file1.dat --- B-T-RC3 B_T from the RC3 number=3 B galaxy magnitudes taken from the RC3. 0.00 = no data. Bytes 40-44 - Observed B_T as given in the computer version of RC3 Bytes 47-51 - Observed m_B as given in computer version of RC3; these are B mags other sources, including ESO catalog. Bytes 54-58 - RC3 B_To, B_T corrected for Galactic extinction (from Burstein-Heiles values), inclination and K-correction. RC3 converts Burstein-Heiles values of E(B-V) to extinction by a ratio of 4.3 (not 4.0 as assumed by Burstein-Heiles). mag B-T-oth B_T from other sources number=3 B galaxy magnitudes taken from the RC3. 0.00 = no data. Bytes 40-44 - Observed B_T as given in the computer version of RC3 Bytes 47-51 - Observed m_B as given in computer version of RC3; these are B mags other sources, including ESO catalog. Bytes 54-58 - RC3 B_To, B_T corrected for Galactic extinction (from Burstein-Heiles values), inclination and K-correction. RC3 converts Burstein-Heiles values of E(B-V) to extinction by a ratio of 4.3 (not 4.0 as assumed by Burstein-Heiles). mag B-T-RC3C B_T_RC3, corrected number=3 B galaxy magnitudes taken from the RC3. 0.00 = no data. Bytes 40-44 - Observed B_T as given in the computer version of RC3 Bytes 47-51 - Observed m_B as given in computer version of RC3; these are B mags other sources, including ESO catalog. Bytes 54-58 - RC3 B_To, B_T corrected for Galactic extinction (from Burstein-Heiles values), inclination and K-correction. RC3 converts Burstein-Heiles values of E(B-V) to extinction by a ratio of 4.3 (not 4.0 as assumed by Burstein-Heiles). mag GLON Galactic longitude deg GLAT Galactic latitude deg Name Galaxy Name number=4 N = NGC (first name preference) I = IC (2nd preference) U = UGC (Nilson 1973) (3rd preference) E = ESO (Lauberts 1982) (3rd preference) Z = Zwicky, field+number (4th preference) A = Anonymous, RA (hr,min), Dec (deg) (4th preference) --- RC3_type RC3 galaxy type code --- Mark 3 1st Mathewson data file Catnum Unique number in Mark 3 MAT catalog number=1 Catnum is a unique number assigned to each galaxy from a given data source in the Mark 3 catalogs. Mathewson Catnum values go from 1 to 1355. --- PGCnum Principal Galaxy Catalog number --- Name Mathewson Name for Galaxy number=2 The name of the galaxy as given by Mathewson et al. E = ESO catalog name, in a format e.g. E539-005 M = MCG catalog name, in a format e.g., M-1-2-14 = M0102014 A = Anonymous galaxy designation, with RA (hr,min) and Dec (deg) given N = NGC number U = UGC number --- RAh 1950 Right Ascension (hour) h RAm 1950 Right Ascension (min) min RAs 1950 Right Ascension (seconds) s DE- Sign of declination --- DEd 1950 Declination (degrees) deg DEm 1950 Declination (arcmin) arcmin DEs 1950 Declination (arcsec) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg HelioV Heliocentric radial velocity number=3 HelioV is the heliocentric radial velocity of the galaxy, as quoted by Mathewson. CMB_V is the radial velocity of the galaxy relative to the Cosmic Microwave Background, as quoted by Mathewson. (This will not, in general, be equal to the CMB velocities given in the individual galaxy distance files, because Mathewson et al. used a different conversion from heliocentric to CMB velocities.) km/s CMB_V Radial velocity w.r.t. CMB number=3 HelioV is the heliocentric radial velocity of the galaxy, as quoted by Mathewson. CMB_V is the radial velocity of the galaxy relative to the Cosmic Microwave Background, as quoted by Mathewson. (This will not, in general, be equal to the CMB velocities given in the individual galaxy distance files, because Mathewson et al. used a different conversion from heliocentric to CMB velocities.) km/s DMaj_MAT Mathewson I band major axis number=4 Bytes 70-73 (DMaj_MAT), 76-79 (DMin_MAT), 81-82 (Incl_MAT), 84-86 (PA_MAT), 89-92 (Lg(a/b)M), 95-98 (LogD_Mat) and 101-104 (LgD_Matc) are all values taken directly from the Mathewson et al. paper for the defined parameters. LogD_Mat is the I band diameter of the galaxy as observed by Mathewson et al. (i.e., before any corrections are applied). LogD_Matc is the I-band diameter as fully-corrected for Galactic extinction, inclination and K-corrections by Mathewson et al., but not the diameter used in the Mark 3 analysis. arcmin DMin_MAT Mathewson I band minor axis number=4 Bytes 70-73 (DMaj_MAT), 76-79 (DMin_MAT), 81-82 (Incl_MAT), 84-86 (PA_MAT), 89-92 (Lg(a/b)M), 95-98 (LogD_Mat) and 101-104 (LgD_Matc) are all values taken directly from the Mathewson et al. paper for the defined parameters. LogD_Mat is the I band diameter of the galaxy as observed by Mathewson et al. (i.e., before any corrections are applied). LogD_Matc is the I-band diameter as fully-corrected for Galactic extinction, inclination and K-corrections by Mathewson et al., but not the diameter used in the Mark 3 analysis. arcmin Incl_MAT Inclination of galaxy as quoted by MAT number=4 Bytes 70-73 (DMaj_MAT), 76-79 (DMin_MAT), 81-82 (Incl_MAT), 84-86 (PA_MAT), 89-92 (Lg(a/b)M), 95-98 (LogD_Mat) and 101-104 (LgD_Matc) are all values taken directly from the Mathewson et al. paper for the defined parameters. LogD_Mat is the I band diameter of the galaxy as observed by Mathewson et al. (i.e., before any corrections are applied). LogD_Matc is the I-band diameter as fully-corrected for Galactic extinction, inclination and K-corrections by Mathewson et al., but not the diameter used in the Mark 3 analysis. deg PA_MAT Mathewson position angle of DMaj_MAT number=4 Bytes 70-73 (DMaj_MAT), 76-79 (DMin_MAT), 81-82 (Incl_MAT), 84-86 (PA_MAT), 89-92 (Lg(a/b)M), 95-98 (LogD_Mat) and 101-104 (LgD_Matc) are all values taken directly from the Mathewson et al. paper for the defined parameters. LogD_Mat is the I band diameter of the galaxy as observed by Mathewson et al. (i.e., before any corrections are applied). LogD_Matc is the I-band diameter as fully-corrected for Galactic extinction, inclination and K-corrections by Mathewson et al., but not the diameter used in the Mark 3 analysis. deg Lg(a/b)M Mathewson value of log (a/b) number=4 Bytes 70-73 (DMaj_MAT), 76-79 (DMin_MAT), 81-82 (Incl_MAT), 84-86 (PA_MAT), 89-92 (Lg(a/b)M), 95-98 (LogD_Mat) and 101-104 (LgD_Matc) are all values taken directly from the Mathewson et al. paper for the defined parameters. LogD_Mat is the I band diameter of the galaxy as observed by Mathewson et al. (i.e., before any corrections are applied). LogD_Matc is the I-band diameter as fully-corrected for Galactic extinction, inclination and K-corrections by Mathewson et al., but not the diameter used in the Mark 3 analysis. --- LogD_Mat Log DMaj_MAT, as observed number=4 Bytes 70-73 (DMaj_MAT), 76-79 (DMin_MAT), 81-82 (Incl_MAT), 84-86 (PA_MAT), 89-92 (Lg(a/b)M), 95-98 (LogD_Mat) and 101-104 (LgD_Matc) are all values taken directly from the Mathewson et al. paper for the defined parameters. LogD_Mat is the I band diameter of the galaxy as observed by Mathewson et al. (i.e., before any corrections are applied). LogD_Matc is the I-band diameter as fully-corrected for Galactic extinction, inclination and K-corrections by Mathewson et al., but not the diameter used in the Mark 3 analysis. .1arcmin LgD_Matc Log DMaj_MAT, fully-corrected, as publ number=4 Bytes 70-73 (DMaj_MAT), 76-79 (DMin_MAT), 81-82 (Incl_MAT), 84-86 (PA_MAT), 89-92 (Lg(a/b)M), 95-98 (LogD_Mat) and 101-104 (LgD_Matc) are all values taken directly from the Mathewson et al. paper for the defined parameters. LogD_Mat is the I band diameter of the galaxy as observed by Mathewson et al. (i.e., before any corrections are applied). LogD_Matc is the I-band diameter as fully-corrected for Galactic extinction, inclination and K-corrections by Mathewson et al., but not the diameter used in the Mark 3 analysis. .1arcmin Extinc_I Galactic Extinction in I-band number=5 Bytes 107-110 (Extinc_I) are I-band extinctions by the relation A_I = 1.68(E(B-V). Values of E(B-V) come from Burstein-Heiles as quoted in the RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). If no RC3 reddening given, then Mathewson value is used. Bytes 112-116 (I_T_MAT1) are the Mathewson observed I band magnitudes corrected only for the values of Extinc_I. In particular, these are not the same corrected I band magnitudes as quoted by Mathewson et al. mag I-T-MAT1 Observed MAT I mag, cor only for Extinc_1 number=5 Bytes 107-110 (Extinc_I) are I-band extinctions by the relation A_I = 1.68(E(B-V). Values of E(B-V) come from Burstein-Heiles as quoted in the RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). If no RC3 reddening given, then Mathewson value is used. Bytes 112-116 (I_T_MAT1) are the Mathewson observed I band magnitudes corrected only for the values of Extinc_I. In particular, these are not the same corrected I band magnitudes as quoted by Mathewson et al. mag Mark 3 2nd Mathewson data file Catnum Unique number in Mark 3 MAT catalog number=1 Catnum is a unique number assigned to each galaxy from a given data source in the Mark 3 catalogs. Mathewson Catnum values go from 1 to 1355. --- Opt_helV Optical Heliocentric radial vel number=2 Bytes 7-11 (Opt_helV) is the heliocentric velocity of the galaxy quoted by Mathewson et al. from optical spectra. Bytes 13-17 (Rad_helV) is the heliocentric velocity of the galaxy quoted by Mathewson et al. from 21 cm HI radio observations. km/s Rad_helV 21 cm Radio Heliocentric radial vel number=2 Bytes 7-11 (Opt_helV) is the heliocentric velocity of the galaxy quoted by Mathewson et al. from optical spectra. Bytes 13-17 (Rad_helV) is the heliocentric velocity of the galaxy quoted by Mathewson et al. from 21 cm HI radio observations. km/s DelV_20 21 cm Delta(V/2), at 20% level number=3 Bytes 20-22 (DelV_20) is the HI velocity profile half-width measured at 20% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 25-27 (DelV_50) is the HI velocity profile half-width measured at 50% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 30-32 (Delv_opt) is the velocity profile half-width as measured from H-alpha emission lines measured from optical spectra. Bytes 35-37 (DelV_MAT) is the velocity profile half-width adopted by Mathewson et al., corrected for THEIR quoted value of galaxy inclination. Byte 38 is given a colon (:) if, in the judgement of Mathewson et al. the quoted DelV_MAT is of lower quality. Bytes 108-112 is the log of DelV_MAT. km/s DelV_50 21 cm Delta(V/2), at 50% level number=3 Bytes 20-22 (DelV_20) is the HI velocity profile half-width measured at 20% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 25-27 (DelV_50) is the HI velocity profile half-width measured at 50% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 30-32 (Delv_opt) is the velocity profile half-width as measured from H-alpha emission lines measured from optical spectra. Bytes 35-37 (DelV_MAT) is the velocity profile half-width adopted by Mathewson et al., corrected for THEIR quoted value of galaxy inclination. Byte 38 is given a colon (:) if, in the judgement of Mathewson et al. the quoted DelV_MAT is of lower quality. Bytes 108-112 is the log of DelV_MAT. km/s Delv_opt H-alpha Delta(V/2) number=3 Bytes 20-22 (DelV_20) is the HI velocity profile half-width measured at 20% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 25-27 (DelV_50) is the HI velocity profile half-width measured at 50% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 30-32 (Delv_opt) is the velocity profile half-width as measured from H-alpha emission lines measured from optical spectra. Bytes 35-37 (DelV_MAT) is the velocity profile half-width adopted by Mathewson et al., corrected for THEIR quoted value of galaxy inclination. Byte 38 is given a colon (:) if, in the judgement of Mathewson et al. the quoted DelV_MAT is of lower quality. Bytes 108-112 is the log of DelV_MAT. km/s DelV_MAT Mathewson adopted Delta(V/2), incl-corr number=3 Bytes 20-22 (DelV_20) is the HI velocity profile half-width measured at 20% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 25-27 (DelV_50) is the HI velocity profile half-width measured at 50% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 30-32 (Delv_opt) is the velocity profile half-width as measured from H-alpha emission lines measured from optical spectra. Bytes 35-37 (DelV_MAT) is the velocity profile half-width adopted by Mathewson et al., corrected for THEIR quoted value of galaxy inclination. Byte 38 is given a colon (:) if, in the judgement of Mathewson et al. the quoted DelV_MAT is of lower quality. Bytes 108-112 is the log of DelV_MAT. km/s f_DelV* Indication if Delta(V/2) error large number=3 Bytes 20-22 (DelV_20) is the HI velocity profile half-width measured at 20% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 25-27 (DelV_50) is the HI velocity profile half-width measured at 50% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 30-32 (Delv_opt) is the velocity profile half-width as measured from H-alpha emission lines measured from optical spectra. Bytes 35-37 (DelV_MAT) is the velocity profile half-width adopted by Mathewson et al., corrected for THEIR quoted value of galaxy inclination. Byte 38 is given a colon (:) if, in the judgement of Mathewson et al. the quoted DelV_MAT is of lower quality. Bytes 108-112 is the log of DelV_MAT. --- HI_flux HI flux, in units of milli-Jy-km/sec mJy*km/s e_HI_flux error in HI flux measurement mJy*km/s Extinc_B Galactic extinction, B-band number=4 Bytes 53-56 (Extinc_B) are values of 4E(B-V), with E(B-V) using the Burstein-Heiles method as quoted in the RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). If no RC3 reddening given, then Mathewson value for Extinc_B is used. mag Bc_RC3 Extinc-corr B_T magnitude from RC3 number=5 Bytes 59-63 (B_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 66-69 (LogD_RC3) and 71-75 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. mag LogD_RC3 Log D_25 from RC3 number=5 Bytes 59-63 (B_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 66-69 (LogD_RC3) and 71-75 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. .1arcmin RC3_axis =-0.99 Log (a/b) from RC3 number=5 Bytes 59-63 (B_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 66-69 (LogD_RC3) and 71-75 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. --- DMaj_ESO ESO eye-determ B band major axis number=6 Bytes 77-81 (DMaj_ESO) and 83-87 (DMin_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 89-93 (Bmag_ELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 95-99 (Rmag_ELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 101-105 (DMaj_ELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). arcmin DMin_ESO ESO eye-determ B band minor axis number=6 Bytes 77-81 (DMaj_ESO) and 83-87 (DMin_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 89-93 (Bmag_ELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 95-99 (Rmag_ELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 101-105 (DMaj_ELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). arcmin Bmag_ELV ESO-LV B-band magnitude number=6 Bytes 77-81 (DMaj_ESO) and 83-87 (DMin_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 89-93 (Bmag_ELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 95-99 (Rmag_ELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 101-105 (DMaj_ELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). mag Rmag_ELV ESO-LV R-band magnitude number=6 Bytes 77-81 (DMaj_ESO) and 83-87 (DMin_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 89-93 (Bmag_ELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 95-99 (Rmag_ELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 101-105 (DMaj_ELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). mag DMaj_ELV ESO-LV B band major axis diameter number=6 Bytes 77-81 (DMaj_ESO) and 83-87 (DMin_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 89-93 (Bmag_ELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 95-99 (Rmag_ELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 101-105 (DMaj_ELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). arcmin LogDelV Log of DelV_MAT number=3 Bytes 20-22 (DelV_20) is the HI velocity profile half-width measured at 20% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 25-27 (DelV_50) is the HI velocity profile half-width measured at 50% of the maximum of HI flux in the profile, as quoted by Mathewson et al. Bytes 30-32 (Delv_opt) is the velocity profile half-width as measured from H-alpha emission lines measured from optical spectra. Bytes 35-37 (DelV_MAT) is the velocity profile half-width adopted by Mathewson et al., corrected for THEIR quoted value of galaxy inclination. Byte 38 is given a colon (:) if, in the judgement of Mathewson et al. the quoted DelV_MAT is of lower quality. Bytes 108-112 is the log of DelV_MAT. km/s Name Mathewson Name for Galaxy number=7 The name of the galaxy as given by Mathewson et al. E = ESO catalog name, in a format e.g. E539-005 M = MCG catalog name, in a format e.g., M-1-2-14 = M0102014 A = Anonymous galaxy designation, with RA (hr,min) and Dec (deg) given N = NGC number U = UGC number --- Mark 3 3rd Mathewson data file Catnum Unique number in Mark 3 MAT catalog number=1 Catnum is a unique number assigned to each galaxy from a given data source in the Mark 3 catalogs. Mathewson Catnum values go from 1 to 1355. --- B-I_cat1 =-9.99 B_RC3 minus I_MAT, extinc-corr number=2 These parameters are galaxy colors determined by taking catalog values of magnitudes and the Mathewson et al. I band magnitude. These values are corrected for Galactic extinction only (i.e., no inclination correction has been applied). Bytes 7-11 (B-I_cat1) is the B-I total magnitude using RC3 B_T and MAT_I. Bytes 13-17 (B-I_cat2) is the B-I total magnitude using ESO-LV B_T and MAT_I. Bytes 19-23 (R-I_cat1) is the R-I total magnitude using ESO-LV R_T and MAT_I. RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). ESO catalog (Lauberts 1982). ESO-LV catalog - Surface Photometry Catalog of the ESO galaxies (Lauberts and Valentijn 1989). mag B-I_cat2 =-9.99 B_ESO-LV minus I_MAT, extinc-corr number=2 These parameters are galaxy colors determined by taking catalog values of magnitudes and the Mathewson et al. I band magnitude. These values are corrected for Galactic extinction only (i.e., no inclination correction has been applied). Bytes 7-11 (B-I_cat1) is the B-I total magnitude using RC3 B_T and MAT_I. Bytes 13-17 (B-I_cat2) is the B-I total magnitude using ESO-LV B_T and MAT_I. Bytes 19-23 (R-I_cat1) is the R-I total magnitude using ESO-LV R_T and MAT_I. RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). ESO catalog (Lauberts 1982). ESO-LV catalog - Surface Photometry Catalog of the ESO galaxies (Lauberts and Valentijn 1989). mag R-I_cat2 =-9.99 R_ESO-LV minus I_MAT, extinc-corr number=2 These parameters are galaxy colors determined by taking catalog values of magnitudes and the Mathewson et al. I band magnitude. These values are corrected for Galactic extinction only (i.e., no inclination correction has been applied). Bytes 7-11 (B-I_cat1) is the B-I total magnitude using RC3 B_T and MAT_I. Bytes 13-17 (B-I_cat2) is the B-I total magnitude using ESO-LV B_T and MAT_I. Bytes 19-23 (R-I_cat1) is the R-I total magnitude using ESO-LV R_T and MAT_I. RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). ESO catalog (Lauberts 1982). ESO-LV catalog - Surface Photometry Catalog of the ESO galaxies (Lauberts and Valentijn 1989). mag LogD_ESO Log Maj axis, ESO eye measures number=3 Bytes 26-29 (LogD_ESO) is the Log of the ESO (Lauberts 1982) eye-estimated major axis diameter, in the usual 0.1 arcmin RC3 format. Bytes 32-35 (LogD_ELV) is the Log of the ESO-LV B mag D_25 major axis diameter, in the usual 0.1 arcmin RC3 format. Bytes 38-41 (Lg(a/b)E) is the log (a/b) of the galaxy as determined from the ESO-LV catalog. .1arcmin LogD_ELV Log Maj axis, ESO_LV number=3 Bytes 26-29 (LogD_ESO) is the Log of the ESO (Lauberts 1982) eye-estimated major axis diameter, in the usual 0.1 arcmin RC3 format. Bytes 32-35 (LogD_ELV) is the Log of the ESO-LV B mag D_25 major axis diameter, in the usual 0.1 arcmin RC3 format. Bytes 38-41 (Lg(a/b)E) is the log (a/b) of the galaxy as determined from the ESO-LV catalog. .1arcmin Lg(a/b)E Log (a/b), ESO-LV measures number=3 Bytes 26-29 (LogD_ESO) is the Log of the ESO (Lauberts 1982) eye-estimated major axis diameter, in the usual 0.1 arcmin RC3 format. Bytes 32-35 (LogD_ELV) is the Log of the ESO-LV B mag D_25 major axis diameter, in the usual 0.1 arcmin RC3 format. Bytes 38-41 (Lg(a/b)E) is the log (a/b) of the galaxy as determined from the ESO-LV catalog. --- D-a/b1 Log(a/b)RC3 minus Log(a/b)MAT number=4 These are differences between the various measures of axial ratios for each galaxy. Bytes 44-48 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_MAT. Bytes 50-54 (D-a/b2) is the difference, log(a/b)_ESO minus Log(a/b)_MAT. Bytes 56-60 (D-a/b3) is the difference, log(a/b)_ESO-LV minus Log(a/b)_MAT. --- D-a/b2 Log(a/b)ESO minus Log(a/b)MAT number=4 These are differences between the various measures of axial ratios for each galaxy. Bytes 44-48 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_MAT. Bytes 50-54 (D-a/b2) is the difference, log(a/b)_ESO minus Log(a/b)_MAT. Bytes 56-60 (D-a/b3) is the difference, log(a/b)_ESO-LV minus Log(a/b)_MAT. --- D-a/b3 Log(a/b)ESO-LV minus Log(a/b)MAT number=4 These are differences between the various measures of axial ratios for each galaxy. Bytes 44-48 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_MAT. Bytes 50-54 (D-a/b2) is the difference, log(a/b)_ESO minus Log(a/b)_MAT. Bytes 56-60 (D-a/b3) is the difference, log(a/b)_ESO-LV minus Log(a/b)_MAT. --- q_Incl MAT inclination quality 1 number=5 Given the problems found with the published Mathewson et al. axial ratios and inclinations, in the Mark3 catalog we have indicated those galaxies which have serious differences in their quoted axial ratios between Mathewson and the other galaxy catalogs. Byte 63: (q_Incl_1) This indicator is 1 if the Mathewson adopted inclination of the galaxy is less than 38 deg (the cutoff for the Mark3 sample). It is 0 otherwise. Byte 65: (q_Incl_2) This parameter results from testing how the quoted Mathewson et al. galaxy inclination compares with taking the value of log(a/b) quoted for the galaxy and determining inclination from that value. If the difference in inclination, abs(MAT minus a/b_inferred) is 4 deg or less, this quality parameter is 0; if the difference is 5-9 deg, it is 1; if the difference is 10-14 deg it is 2; if the difference is 15 deg or greater, it is 3. Byte 71 (q_Incl_3) This parameter tests for consistency between the axial ratio of the galaxy as given by the RC3 and that given by MAT. If the value in Bytes 44-48 (Diff_a/b1) is 0.30 or greater, this means strong disagreement in axial ratio measurements, and this parameter is 1. Otherwise, this parameter is zero. --- q_Incl2 MAT inclination quality 2 number=5 Given the problems found with the published Mathewson et al. axial ratios and inclinations, in the Mark3 catalog we have indicated those galaxies which have serious differences in their quoted axial ratios between Mathewson and the other galaxy catalogs. Byte 63: (q_Incl_1) This indicator is 1 if the Mathewson adopted inclination of the galaxy is less than 38 deg (the cutoff for the Mark3 sample). It is 0 otherwise. Byte 65: (q_Incl_2) This parameter results from testing how the quoted Mathewson et al. galaxy inclination compares with taking the value of log(a/b) quoted for the galaxy and determining inclination from that value. If the difference in inclination, abs(MAT minus a/b_inferred) is 4 deg or less, this quality parameter is 0; if the difference is 5-9 deg, it is 1; if the difference is 10-14 deg it is 2; if the difference is 15 deg or greater, it is 3. Byte 71 (q_Incl_3) This parameter tests for consistency between the axial ratio of the galaxy as given by the RC3 and that given by MAT. If the value in Bytes 44-48 (Diff_a/b1) is 0.30 or greater, this means strong disagreement in axial ratio measurements, and this parameter is 1. Otherwise, this parameter is zero. --- q_DelV Indication of low Delta(V/2) number=6 Byte 67: (q_DelV) This parameter is zero if log (DeltaV/2) is 1.90 or greater (that is, rotation velocity 79 km/sec or more); it is 1 if log (DeltaV/2) is less than 1.90. --- f_type Indication of peculiar RC3_type number=7 Byte 69 (f_type) This parameter is 1 if the Hubble type given in the RC3 includes the parameter P in such a way that the galaxy is identified as being peculiar. The parameter is two if there is no magnitude for the galaxy in either the RC3 or ESO-LV catalogs. The parameter is zero otherwise. --- q_Incl_3 MAT inclination quality 3 number=5 Given the problems found with the published Mathewson et al. axial ratios and inclinations, in the Mark3 catalog we have indicated those galaxies which have serious differences in their quoted axial ratios between Mathewson and the other galaxy catalogs. Byte 63: (q_Incl_1) This indicator is 1 if the Mathewson adopted inclination of the galaxy is less than 38 deg (the cutoff for the Mark3 sample). It is 0 otherwise. Byte 65: (q_Incl_2) This parameter results from testing how the quoted Mathewson et al. galaxy inclination compares with taking the value of log(a/b) quoted for the galaxy and determining inclination from that value. If the difference in inclination, abs(MAT minus a/b_inferred) is 4 deg or less, this quality parameter is 0; if the difference is 5-9 deg, it is 1; if the difference is 10-14 deg it is 2; if the difference is 15 deg or greater, it is 3. Byte 71 (q_Incl_3) This parameter tests for consistency between the axial ratio of the galaxy as given by the RC3 and that given by MAT. If the value in Bytes 44-48 (Diff_a/b1) is 0.30 or greater, this means strong disagreement in axial ratio measurements, and this parameter is 1. Otherwise, this parameter is zero. --- DB_type Burstein numerical morphological type number=8 Bytes 73-75 (DB_type) Burstein developed a hierarchical numerical typing system for Morphological types. The system for the RC3, ESO and UGC catalogs is as follows: Burstein Code Number Classification 10 Ellipticals - normal 11 E - cD or '+' in RC3 12 Compact E's in RC3 14 E? in RC3 15 E-S0 100 S0 101 SB0 110 S0/a 111 SB0/a 120 Sa 121 SBa 122 Sa/SBa 130 Sa/b 131 SBa/b 132 Sa/b/SBa/b 140 Sb 141 SBb 142 Sb/SBb 150 Sb/Sc 151 SBb/c 152 Sb/c/SBb/c 160 Sc 161 SBc 162 Sc/SBc 170 Sc/d 171 SBc/d 172 Sc/d/SBc/d 180 Sd 181 SBd 190 Sd/Irr 191 SBd/Irr 192 SABd/Irr 195 Im 196 IBm 197 IABm 200 Irr 201 Dwarf Irr 210 Irregular labeled 'P' in RC3 (3 galaxies) 300 'S' 305 'SB' 310 'I?','IB?" 350 'L?' 400 Dwarf 500 Compacts 510 N 600 Multiple galaxies 610 Compact groups 620 Clusters 650 Doubles (general) 651 Doubles: E+E, E+S0, S0+S0 652 Doubles: E+S, S0+S 700 Peculiar 900 No galaxy class given If one takes the numerical type and divides by 10 and take the integer result, one gets: Code Number/10 General Classification 1 E and E/S0 10 All S0 11 All S0/a 12 All Sa 13 All Sa/b 14 All Sb 15 All Sb/Sc 16 All Sc 17 All Sc/Sd 18 All Sd 19 All Sd/Irr 20 All Irr 30 All non-divided classified types 40 Dwarf galaxies 50 Compact galaxies and N galaxies 60 Multiple systems 70 Peculiar galaxies 90 No galaxy class given Separately, one can test for SB, and S/SB galaxies by an appropriate manipulation of the code number. In this way, most of the detail in the morphological classification can be used in a numerical manner. --- RC3_type Morphological type from RC3 --- ESO_type Morphological type from ESO --- Mark 3 Willick 1991 data_1 file RC3num Number in computer-readable RC3 file number=1 RC3num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following three catalogs, as stored in Ultrix format by Burstein. UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than original UGC, owing to inclusion of some UGCA objects. Also, many typos in original computer version have been corrected in this version. The actual UGC number can differ from the storage number UGCnum, owing to the extra galaxies in the computer-readable UGC catalog. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. (There are no ESO galaxies in the W91 sample.) --- UGCnum Number in computer-readable UGC file number=1 RC3num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following three catalogs, as stored in Ultrix format by Burstein. UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than original UGC, owing to inclusion of some UGCA objects. Also, many typos in original computer version have been corrected in this version. The actual UGC number can differ from the storage number UGCnum, owing to the extra galaxies in the computer-readable UGC catalog. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. (There are no ESO galaxies in the W91 sample.) --- ESOnum Number in computer-readable ESO file number=1 RC3num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following three catalogs, as stored in Ultrix format by Burstein. UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than original UGC, owing to inclusion of some UGCA objects. Also, many typos in original computer version have been corrected in this version. The actual UGC number can differ from the storage number UGCnum, owing to the extra galaxies in the computer-readable UGC catalog. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. (There are no ESO galaxies in the W91 sample.) --- PGCnum Principal Galaxy Catalog number --- Catnum Unique number in Mark 3 W91 catalog number=2 Bytes 25-28 (Catnum) is a record number uniquely assigned to each Willick 1991 galaxy in the Mark III analysis. Willick Catnum values from 1 to 383 are the Perseus-Pisces (W91PP) sample; Willick Catnum values 384 to 539 are the Willick cluster (W91CL) galaxies. There are 26 galaxies in common between these two Willick samples: Catnum1 Catnum2 UGC Name 68 384 U00501 71 385 U00525 73 386 U00540 77 387 U00556 78 388 U00557 79 389 U00562 81 390 U00565 84 392 U00624 85 393 U00633 90 394 U00679 93 395 U00732 96 396 U00810 97 397 U00820 98 398 U00841 102 399 U00927 106 400 U00987 107 401 U01013 113 402 U01094 308 503 U12631 317 504 U12678 319 505 U12701 321 506 U12721 324 507 U12746 326 508 U12755 329 509 U12772 335 510 U12855 In addition, there are 57 Willick galaxies in the DATA (w91filex.lst) files that are not given distances in the mark3_ind* files. 40 of these galaxies are the Zwicky galaxies, which are not part of the UGC-diameter limited, complete sample used in the Mark III analysis papers (see Willick et al. 1996). 17 UGC galaxies were also excluded based on excessively large apparent peculiar velocities, indicating either bad magnitudes, bad inclination or bad HI velocity profile width. The 17 UGC galaxies excluded are given here: Catnum UGC Name (Galaxy excluded from distance files) 31 U00208 80 U00564 86 U00645 124 U01277 135 U01456 141 U01550 179 U01935 183 U01963 195 U02079 199 U02183 233 U12025 237 U12059 294 U12546 315 U12672 330 U12780 341 U12914 342 U12915 --- Name Name assigned galaxy by Willick number=3 N = NGC I = IC U = UGC (Nilson 1973) E = ESO (Lauberts 1982) C = Zwicky, field+number A = Anonymous, RA (hr,min), Dec (deg) --- RAh =-99.000 1950 RA, in decimal hours number=4 Coordinates are expressed in decimal numbers. RA is in hour, declination in degrees. To convert RA to standard hr,min,sec, one must successively convert the decimal part of this number to min and sec. Similarly for declination. h DEd =-99.000 1950 Declination, decimal deg. number=4 Coordinates are expressed in decimal numbers. RA is in hour, declination in degrees. To convert RA to standard hr,min,sec, one must successively convert the decimal part of this number to min and sec. Similarly for declination. deg GLON Galactic longitude deg GLAT Galactic latitude deg HelioV Heliocentric radial velocity number=5 Bytes 69-74 (HelioV) is the heliocentric radial velocity of the galaxy, from sources as quoted by Willick (1991, Ph.D. thesis) Bytes 76-81 (CMB_V) is the radial velocity of the galaxy relative to the Cosmic Microwave Background, using the COBE heliocentric-to-CMB correction of 368.6 km/sec towards l=264.7deg, b=48.2deg. km/s CMB_V Radial velocity w.r.t. CMB number=5 Bytes 69-74 (HelioV) is the heliocentric radial velocity of the galaxy, from sources as quoted by Willick (1991, Ph.D. thesis) Bytes 76-81 (CMB_V) is the radial velocity of the galaxy relative to the Cosmic Microwave Background, using the COBE heliocentric-to-CMB correction of 368.6 km/sec towards l=264.7deg, b=48.2deg. km/s Inclin Inclination of galaxy as quoted by W91 deg Log(a/b) Log of axial ratio, obs by W91 --- Extinc_r Galactic Extinction in r-band number=6 Bytes 96-99 (Extinc_r): Burstein-Heiles reddenings E(B-V), converted to r-band extinctions by the relation A_r = 2.24(E(B-V) as derived by Courteau (1996, ApJ Suppl. 103, p. 363) for r band data. mag w91_rmag Galaxy total r mag, as observed number=7 Bytes 101-105 (w91_rmag) is the total extrapolated r magnitude for the galaxy, as observed. w91rmagc (bytes 107-111) is the corrected total magnitude obtained by subtracting the correction Extinc_r (bytes 96-99) from w91_rmag. mag w91rmagc w91_rmag corrected for Extinc_r only number=7 Bytes 101-105 (w91_rmag) is the total extrapolated r magnitude for the galaxy, as observed. w91rmagc (bytes 107-111) is the corrected total magnitude obtained by subtracting the correction Extinc_r (bytes 96-99) from w91_rmag. mag Mark 3 Willick 1991 data_2 file Catnum Unique number in Mark 3 W91 catalog number=1 Catnum is a record number uniquely assigned to each Willick 1991 galaxy in the Mark III analysis. Willick Catnum values from 1 to 383 are the Perseus-Pisces (W91PP) sample; Willick Catnum values 384 to 539 are the Willick cluster (W91CL) galaxies. See Note (2) for file w91file1.lst for further information. --- Radial_V CMB frame radial velocity from W91 km/s DelV_cor 21 cm Delta(V), inclination-corrected number=2 Bytes 15-17 (DelV_cor) is the HI velocity width profile, corrected for internal velocity dispersion as given in the Han, Mould et al. paper. Bytes 20-22 (DelV_obs) is the HI velocity width profile, as observed. Bytes 50-54 (LDelVw91) is the logarithm of DelV_cor. km/s DelV_obs 21 cm Delta(V), as observed number=2 Bytes 15-17 (DelV_cor) is the HI velocity width profile, corrected for internal velocity dispersion as given in the Han, Mould et al. paper. Bytes 20-22 (DelV_obs) is the HI velocity width profile, as observed. Bytes 50-54 (LDelVw91) is the logarithm of DelV_cor. km/s Extinc_B Galactic extinction, B-band number=3 Bytes 25-28 (Extinc_B) are values of 4E(B-V), with E(B-V) using the Burstein-Heiles method as quoted in the RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). If galaxy not in RC3, E(B-V) taken from either UGC or ESO computer catalogs of Burstein having Burstein-Heiles reddenings, or calculated directly from the Burstein-Heiles computer-readable reddening maps. mag Bc_RC3 =-9.99 Extinc-corr B_T mag from RC3 number=4 Bytes 31-35 (Bc_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 38-41 (LogD_RC3) and 44-47 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. mag LogD_RC3 Log D_25 from RC3 number=4 Bytes 31-35 (Bc_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 38-41 (LogD_RC3) and 44-47 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. .1arcmin RC3_axis =-0.99 Log (a/b) from RC3 number=4 Bytes 31-35 (Bc_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 38-41 (LogD_RC3) and 44-47 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. --- LDelVw91 Log of DelV_cor number=2 Bytes 15-17 (DelV_cor) is the HI velocity width profile, corrected for internal velocity dispersion as given in the Han, Mould et al. paper. Bytes 20-22 (DelV_obs) is the HI velocity width profile, as observed. Bytes 50-54 (LDelVw91) is the logarithm of DelV_cor. km/s Name UGC number or Zwicky (C) fld+numb for galaxy --- Mark 3 Willick 1991 data_3 file Catnum Unique number in Mark 3 W91 catalog number=1 Catnum is a record number uniquely assigned to each Willick 1991 galaxy in the Mark III analysis. Willick Catnum values from 1 to 383 are the Perseus-Pisces (W91PP) sample; Willick Catnum values 384 to 539 are the Willick cluster (W91CL) galaxies. See Note (2) for file w91file1.lst for further information. --- B-r_cat1 =-9.99 B_RC3 minus r_W91, extinc-corr number=2 Bytes 7-11 (B-r_cat1) is the B-r color using RC3 B_T and r_w91. RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). mag D-a/b1 Log(a/b)RC3 minus Log(a/b)w91 number=3 These are differences between the various measures of axial ratios for each galaxy. Bytes 13-17 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_W91. Bytes 19-23 (D-a/b4) is the difference, log(a/b)_UGC minus Log(a/b)_W91. --- D-a/b4 Log(a/b)UGC minus Log(a/b)w91 number=3 These are differences between the various measures of axial ratios for each galaxy. Bytes 13-17 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_W91. Bytes 19-23 (D-a/b4) is the difference, log(a/b)_UGC minus Log(a/b)_W91. --- f_type Indication of peculiar RC3_type number=4 Byte 25 (f_type) This parameter is one if the Hubble type given in the RC3 includes the parameter P in such a way that the galaxy is identified as being peculiar, an S0 or an S0/a. The parameter is zero otherwise. --- q_Incl_3 W91 inclination quality 1 number=5 Byte 27 (q_Incl_3) This parameter tests for consistency between the axial ratio of the galaxy as given by the RC3 and that given by W91. If the value in Bytes 13-17 (D-a/b1) is 0.30 or greater, this means strong disagreement in axial ratio measurements, and this parameter is one. Otherwise, this parameter is zero. --- DB_type1 Burstein numeral morph type from RC3 number=6 Bytes 29-31 (DB_type1) and bytes 33-35 (DB_type2) Burstein developed a hierarchical numerical typing system for Morphological types. The system for the RC3, ESO and UGC catalogs follows. DB_type1 is the numerical code given to the RC3 morphological type; DB_type2 is the numerical code given to the morphological type from the UGC catalog (UGC types are only given by numerical code.) Burstein Code Number Classification 10 Ellipticals - normal 11 E - cD or '+' in RC3 12 Compact E's in RC3 14 E? in RC3 15 E-S0 100 S0 101 SB0 110 S0/a 111 SB0/a 120 Sa 121 SBa 122 Sa/SBa 130 Sa/b 131 SBa/b 132 Sa/b/SBa/b 140 Sb 141 SBb 142 Sb/SBb 150 Sb/Sc 151 SBb/c 152 Sb/c/SBb/c 160 Sc 161 SBc 162 Sc/SBc 170 Sc/d 171 SBc/d 172 Sc/d/SBc/d 180 Sd 181 SBd 190 Sd/Irr 191 SBd/Irr 192 SABd/Irr 195 Im 196 IBm 197 IABm 200 Irr 201 Dwarf Irr 210 Irregular labeled 'P' in RC3 (3 galaxies) 300 'S' 305 'SB' 310 'I?','IB?" 350 'L?' 400 Dwarf 500 Compacts 510 N 600 Multiple galaxies 610 Compact groups 620 Clusters 650 Doubles (general) 651 Doubles: E+E, E+S0, S0+S0 652 Doubles: E+S, S0+S 700 Peculiar 900 No galaxy class given If one takes the numerical type and divides by 10 and take the integer result, one gets: Code Number/10 General Classification 1 E and E/S0 10 All S0 11 All S0/a 12 All Sa 13 All Sa/b 14 All Sb 15 All Sb/Sc 16 All Sc 17 All Sc/Sd 18 All Sd 19 All Sd/Irr 20 All Irr 30 All non-divided classified types 40 Dwarf galaxies 50 Compact galaxies and N galaxies 60 Multiple systems 70 Peculiar galaxies 90 No galaxy class given Separately, one can test for SB, and S/SB galaxies by an appropriate manipulation of the code number. In this way, most of the detail in the morphological classification can be used in a numerical manner. --- DB_type2 Burstein numerical morph type, UGC number=6 Bytes 29-31 (DB_type1) and bytes 33-35 (DB_type2) Burstein developed a hierarchical numerical typing system for Morphological types. The system for the RC3, ESO and UGC catalogs follows. DB_type1 is the numerical code given to the RC3 morphological type; DB_type2 is the numerical code given to the morphological type from the UGC catalog (UGC types are only given by numerical code.) Burstein Code Number Classification 10 Ellipticals - normal 11 E - cD or '+' in RC3 12 Compact E's in RC3 14 E? in RC3 15 E-S0 100 S0 101 SB0 110 S0/a 111 SB0/a 120 Sa 121 SBa 122 Sa/SBa 130 Sa/b 131 SBa/b 132 Sa/b/SBa/b 140 Sb 141 SBb 142 Sb/SBb 150 Sb/Sc 151 SBb/c 152 Sb/c/SBb/c 160 Sc 161 SBc 162 Sc/SBc 170 Sc/d 171 SBc/d 172 Sc/d/SBc/d 180 Sd 181 SBd 190 Sd/Irr 191 SBd/Irr 192 SABd/Irr 195 Im 196 IBm 197 IABm 200 Irr 201 Dwarf Irr 210 Irregular labeled 'P' in RC3 (3 galaxies) 300 'S' 305 'SB' 310 'I?','IB?" 350 'L?' 400 Dwarf 500 Compacts 510 N 600 Multiple galaxies 610 Compact groups 620 Clusters 650 Doubles (general) 651 Doubles: E+E, E+S0, S0+S0 652 Doubles: E+S, S0+S 700 Peculiar 900 No galaxy class given If one takes the numerical type and divides by 10 and take the integer result, one gets: Code Number/10 General Classification 1 E and E/S0 10 All S0 11 All S0/a 12 All Sa 13 All Sa/b 14 All Sb 15 All Sb/Sc 16 All Sc 17 All Sc/Sd 18 All Sd 19 All Sd/Irr 20 All Irr 30 All non-divided classified types 40 Dwarf galaxies 50 Compact galaxies and N galaxies 60 Multiple systems 70 Peculiar galaxies 90 No galaxy class given Separately, one can test for SB, and S/SB galaxies by an appropriate manipulation of the code number. In this way, most of the detail in the morphological classification can be used in a numerical manner. --- RC3_type Morphological type from RC3 --- Mark 3 Courteau-Faber data_1 file RC3num Number in computer-readable RC3 file number=1 RC3num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following three catalogs, as stored in Ultrix format by Burstein. UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. Name - Here the Name is the UGC number of the galaxy. The actual UGC number can differ from the storage number UGCnum, owing to the extra galaxies in the computer-readable UGC catalog. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. (There are no ESO galaxies in the CF sample.) Likewise, Catnum is a record number uniquely assigned to each Courteau-Faber galaxy in the Mark III analysis. The five Zwicky-only galaxies in this list do not appear in the distance file "mark3_cf_s". These galaxies are: Catnum Zwicky Number 322 C406031 323 C421011 324 C421030 325 C476112 326 C477024 --- UGCnum Number in computer-readable UGC file number=1 RC3num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following three catalogs, as stored in Ultrix format by Burstein. UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. Name - Here the Name is the UGC number of the galaxy. The actual UGC number can differ from the storage number UGCnum, owing to the extra galaxies in the computer-readable UGC catalog. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. (There are no ESO galaxies in the CF sample.) Likewise, Catnum is a record number uniquely assigned to each Courteau-Faber galaxy in the Mark III analysis. The five Zwicky-only galaxies in this list do not appear in the distance file "mark3_cf_s". These galaxies are: Catnum Zwicky Number 322 C406031 323 C421011 324 C421030 325 C476112 326 C477024 --- ESOnum Number in computer-readable ESO file number=1 RC3num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following three catalogs, as stored in Ultrix format by Burstein. UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. Name - Here the Name is the UGC number of the galaxy. The actual UGC number can differ from the storage number UGCnum, owing to the extra galaxies in the computer-readable UGC catalog. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. (There are no ESO galaxies in the CF sample.) Likewise, Catnum is a record number uniquely assigned to each Courteau-Faber galaxy in the Mark III analysis. The five Zwicky-only galaxies in this list do not appear in the distance file "mark3_cf_s". These galaxies are: Catnum Zwicky Number 322 C406031 323 C421011 324 C421030 325 C476112 326 C477024 --- PGCnum Principal Galaxy Catalog number --- Catnum Unique number in Mark 3 CF catalog number=1 RC3num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following three catalogs, as stored in Ultrix format by Burstein. UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. Name - Here the Name is the UGC number of the galaxy. The actual UGC number can differ from the storage number UGCnum, owing to the extra galaxies in the computer-readable UGC catalog. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. (There are no ESO galaxies in the CF sample.) Likewise, Catnum is a record number uniquely assigned to each Courteau-Faber galaxy in the Mark III analysis. The five Zwicky-only galaxies in this list do not appear in the distance file "mark3_cf_s". These galaxies are: Catnum Zwicky Number 322 C406031 323 C421011 324 C421030 325 C476112 326 C477024 --- Name UGC Number or Zwicky number number=1 RC3num, UGCnum and ESOnum are the record numbers for each galaxy in the direct access versions of the following three catalogs, as stored in Ultrix format by Burstein. UGCnum galaxies have Burstein-Heiles galaxy counts and HI measures, from which reddenings can be calculated. RC3num and ESOnum have reddenings alone listed. RC3num - RC3 (de Vaucouleurs et al. 1991), as electronically distributed by Harold Corwin (rc39.all version) UGCnum - Uppsala General Catalogue (Nilson 1973); original version from Ohio State, pre-1980. This direct access catalog has 23 more objects than in original UGC, owing to inclusion of some UGCA objects. Also, many errors in original computer version have been corrected in this version. Name - Here the Name is the UGC number of the galaxy. The actual UGC number can differ from the storage number UGCnum, owing to the extra galaxies in the computer-readable UGC catalog. ESOnum - European Southern Observatory catalog. Culled from the full ESO catalog (Lauberts 1982) for only galaxy or galaxy(?) objects, 16,154 in all. Global ESO-LV (Lauberts-Valentijn 1989) data added to catalog for 14,083 galaxies in common. (There are no ESO galaxies in the CF sample.) Likewise, Catnum is a record number uniquely assigned to each Courteau-Faber galaxy in the Mark III analysis. The five Zwicky-only galaxies in this list do not appear in the distance file "mark3_cf_s". These galaxies are: Catnum Zwicky Number 322 C406031 323 C421011 324 C421030 325 C476112 326 C477024 --- RAh 1950 Right Ascension, in decimal hours number=2 Coordinates are expressed in decimal numbers. RA is in hour, declination in degrees. To convert RA to standard hr,min,sec, one must successively convert the decimal part of this number to min and sec. Similarly for declination. h DEd 1950 Declination, in decimal degrees number=2 Coordinates are expressed in decimal numbers. RA is in hour, declination in degrees. To convert RA to standard hr,min,sec, one must successively convert the decimal part of this number to min and sec. Similarly for declination. deg GLON Galactic longitude deg GLAT Galactic latitude deg HelioV Heliocentric radial velocity number=3 Bytes 68-74 (HelioV) is the heliocentric radial velocity of the galaxy, from sources as quoted by Courteau (1996, ApJ Suppl. 103, p. 363). Bytes 75-81 (CMB_V) is the radial velocity of the galaxy relative to the Cosmic Microwave Background, using the COBE heliocentric-to-CMB correction of 368.6 km/sec towards l=264.7deg, b=48.2deg. km/s CMB_V Radial velocity w.r.t. CMB number=3 Bytes 68-74 (HelioV) is the heliocentric radial velocity of the galaxy, from sources as quoted by Courteau (1996, ApJ Suppl. 103, p. 363). Bytes 75-81 (CMB_V) is the radial velocity of the galaxy relative to the Cosmic Microwave Background, using the COBE heliocentric-to-CMB correction of 368.6 km/sec towards l=264.7deg, b=48.2deg. km/s Inclin Inclination of galaxy as quoted by CF deg Log(a/b) Log of axial ratio, obs by CF --- Extinc_r Galactic Extinction in r-band number=4 Bytes 96-99 (Extinc_r): Burstein-Heiles reddenings E(B-V), converted to r-band extinctions by the relation A_r = 2.24(E(B-V) as assumed by Courteau (1996). mag CF_rmag Galaxy total r mag, as observed number=5 Bytes 101-105 (CF_rmag) is the total extrapolated r magnitude for the galaxy, as observed. CF_rmagc (bytes 107-111) is the corrected total magnitude obtained by subtracting the correction Extinc_r (bytes 96-99) from CF_rmag. mag CF_rmagc CF_rmag corrected for Extinc_r only number=5 Bytes 101-105 (CF_rmag) is the total extrapolated r magnitude for the galaxy, as observed. CF_rmagc (bytes 107-111) is the corrected total magnitude obtained by subtracting the correction Extinc_r (bytes 96-99) from CF_rmag. mag Mark 3 Courteau-Faber data_2 file Catnum Unique number in Mark 3 CF catalog number=1 Catnum is a record number uniquely assigned to each CF galaxy. --- CMB_V Radial velocity w.r.t. CMB number=2 Bytes 7-12 (CMB_V) is the radial velocity of the galaxy relative to the Cosmic Microwave Background, using the COBE heliocentric-to-CMB correction of 368.6 km/sec towards l=264.7deg, b=48.2deg. km/s DelV_cor optical Delta(V), inclination-corrected number=3 Bytes 15-17 (DelV_cor) is the optical velocity width, obtained as described by Courteau (1992, Ph.D. thesis, University of California, Santa Cruz). Bytes 20-22 (DelV_obs) Optical velocity width profile, as observed (Courteau 1992). Bytes 50-54 (LgDelVCF) is the logarithm of DelV_cor. km/s DelV_obs optical Delta(V), as observed number=3 Bytes 15-17 (DelV_cor) is the optical velocity width, obtained as described by Courteau (1992, Ph.D. thesis, University of California, Santa Cruz). Bytes 20-22 (DelV_obs) Optical velocity width profile, as observed (Courteau 1992). Bytes 50-54 (LgDelVCF) is the logarithm of DelV_cor. km/s Extinc_B Galactic extinction, B-band number=4 Bytes 25-28 (Extinc_B) are values of 4E(B-V), with E(B-V) using the Burstein-Heiles method as quoted in the RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). If galaxy not in RC3, E(B-V) taken from either UGC or ESO computer catalogs of Burstein having Burstein-Heiles reddenings, or calculated directly from the Burstein-Heiles computer-readable reddening maps. mag Bc_RC3 =-9.99 Extinc-corr B_T mag from RC3 number=5 Bytes 31-35 (Bc_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction, not for internal extinction. Bytes 38-41 (LogD_RC3) and 44-47 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. The five Zwicky-only galaxies in this list do not appear in the distance file "mark3_cf_s". These galaxies are: Catnum Zwicky Number 322 C406031 323 C421011 324 C421030 325 C476112 326 C477024 mag LogD_RC3 Log D_25 from RC3 number=5 Bytes 31-35 (Bc_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction, not for internal extinction. Bytes 38-41 (LogD_RC3) and 44-47 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. The five Zwicky-only galaxies in this list do not appear in the distance file "mark3_cf_s". These galaxies are: Catnum Zwicky Number 322 C406031 323 C421011 324 C421030 325 C476112 326 C477024 .1arcmin RC3_axis =-0.99 Log (a/b) from RC3 number=5 Bytes 31-35 (Bc_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction, not for internal extinction. Bytes 38-41 (LogD_RC3) and 44-47 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. The five Zwicky-only galaxies in this list do not appear in the distance file "mark3_cf_s". These galaxies are: Catnum Zwicky Number 322 C406031 323 C421011 324 C421030 325 C476112 326 C477024 --- LgDelVCF Log of DelV_cor number=3 Bytes 15-17 (DelV_cor) is the optical velocity width, obtained as described by Courteau (1992, Ph.D. thesis, University of California, Santa Cruz). Bytes 20-22 (DelV_obs) Optical velocity width profile, as observed (Courteau 1992). Bytes 50-54 (LgDelVCF) is the logarithm of DelV_cor. km/s Name UGC number or Zwicky (C) fld+numb for galaxy --- Mark 3 Courteau-Faber data_3 file Catnum Unique number in Mark 3 CF catalog number=1 Catnum is a record number uniquely assigned to each CF galaxy. --- B-r_cat1 =-9.99 B_RC3 minus r_CF, extinc-corr number=2 Bytes 7-11 (B-r_cat1) is the B-r color using RC3 B_T and r_CF. RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). mag D-a/b1 Log(a/b)RC3 minus Log(a/b)CF number=3 These are differences between the various measures of axial ratios for each galaxy. Bytes 13-17 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_CF. Bytes 19-23 (D-a/b4) is the difference, log(a/b)_UGC minus Log(a/b)_CF. --- D-a/b4 Log(a/b)UGC minus Log(a/b)CF number=3 These are differences between the various measures of axial ratios for each galaxy. Bytes 13-17 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_CF. Bytes 19-23 (D-a/b4) is the difference, log(a/b)_UGC minus Log(a/b)_CF. --- f_type Indication of peculiar RC3_type number=4 Byte 25 (f_type) This parameter is 1 if the Hubble type given in the RC3 includes the parameter P in such a way that the galaxy is identified as being peculiar, an S0 or an S0/a. The parameter is zero otherwise. --- q_Incl_3 CF inclination quality 1 number=5 Byte 27 (q_Incl_3) This parameter tests for consistency between the axial ratio of the galaxy as given by the RC3 and that given by CF. If the value in Bytes 13-17 (D-a/b1) is 0.30 or greater, this means strong disagreement in axial ratio measurements, and this parameter is one. Otherwise, this parameter is zero. --- DB_type1 Burstein numerical morph type from RC3 number=6 Bytes 29-31 (DB_type1) and bytes 33-35 (DB_type2) Burstein developed a hierarchical numerical typing system for Morphological types. The system for the RC3, ESO and UGC catalogs follows. DB_type1 is the numerical code given to the RC3 morphological type; DB_type2 is the numerical code given to the morphological type from the ESO catalog (UGC types are only given by numerical code.) Burstein Code Number Classification 10 Ellipticals - normal 11 E - cD or '+' in RC3 12 Compact E's in RC3 14 E? in RC3 15 E-S0 100 S0 101 SB0 110 S0/a 111 SB0/a 120 Sa 121 SBa 122 Sa/SBa 130 Sa/b 131 SBa/b 132 Sa/b/SBa/b 140 Sb 141 SBb 142 Sb/SBb 150 Sb/Sc 151 SBb/c 152 Sb/c/SBb/c 160 Sc 161 SBc 162 Sc/SBc 170 Sc/d 171 SBc/d 172 Sc/d/SBc/d 180 Sd 181 SBd 190 Sd/Irr 191 SBd/Irr 192 SABd/Irr 195 Im 196 IBm 197 IABm 200 Irr 201 Dwarf Irr 210 Irregular labeled 'P' in RC3 (3 galaxies) 300 'S' 305 'SB' 310 'I?','IB?" 350 'L?' 400 Dwarf 500 Compacts 510 N 600 Multiple galaxies 610 Compact groups 620 Clusters 650 Doubles (general) 651 Doubles: E+E, E+S0, S0+S0 652 Doubles: E+S, S0+S 700 Peculiar 900 No galaxy class given If one takes the numerical type and divides by 10 and take the integer result, one gets: Code Number/10 General Classification 1 E and E/S0 10 All S0 11 All S0/a 12 All Sa 13 All Sa/b 14 All Sb 15 All Sb/Sc 16 All Sc 17 All Sc/Sd 18 All Sd 19 All Sd/Irr 20 All Irr 30 All non-divided classified types 40 Dwarf galaxies 50 Compact galaxies and N galaxies 60 Multiple systems 70 Peculiar galaxies 90 No galaxy class given Separately, one can test for SB, and S/SB galaxies by an appropriate manipulation of the code number. In this way, most of the detail in the morphological classification can be used in a numerical manner. --- DB_type2 Burstein numerical morph type, UGC or ESO number=6 Bytes 29-31 (DB_type1) and bytes 33-35 (DB_type2) Burstein developed a hierarchical numerical typing system for Morphological types. The system for the RC3, ESO and UGC catalogs follows. DB_type1 is the numerical code given to the RC3 morphological type; DB_type2 is the numerical code given to the morphological type from the ESO catalog (UGC types are only given by numerical code.) Burstein Code Number Classification 10 Ellipticals - normal 11 E - cD or '+' in RC3 12 Compact E's in RC3 14 E? in RC3 15 E-S0 100 S0 101 SB0 110 S0/a 111 SB0/a 120 Sa 121 SBa 122 Sa/SBa 130 Sa/b 131 SBa/b 132 Sa/b/SBa/b 140 Sb 141 SBb 142 Sb/SBb 150 Sb/Sc 151 SBb/c 152 Sb/c/SBb/c 160 Sc 161 SBc 162 Sc/SBc 170 Sc/d 171 SBc/d 172 Sc/d/SBc/d 180 Sd 181 SBd 190 Sd/Irr 191 SBd/Irr 192 SABd/Irr 195 Im 196 IBm 197 IABm 200 Irr 201 Dwarf Irr 210 Irregular labeled 'P' in RC3 (3 galaxies) 300 'S' 305 'SB' 310 'I?','IB?" 350 'L?' 400 Dwarf 500 Compacts 510 N 600 Multiple galaxies 610 Compact groups 620 Clusters 650 Doubles (general) 651 Doubles: E+E, E+S0, S0+S0 652 Doubles: E+S, S0+S 700 Peculiar 900 No galaxy class given If one takes the numerical type and divides by 10 and take the integer result, one gets: Code Number/10 General Classification 1 E and E/S0 10 All S0 11 All S0/a 12 All Sa 13 All Sa/b 14 All Sb 15 All Sb/Sc 16 All Sc 17 All Sc/Sd 18 All Sd 19 All Sd/Irr 20 All Irr 30 All non-divided classified types 40 Dwarf galaxies 50 Compact galaxies and N galaxies 60 Multiple systems 70 Peculiar galaxies 90 No galaxy class given Separately, one can test for SB, and S/SB galaxies by an appropriate manipulation of the code number. In this way, most of the detail in the morphological classification can be used in a numerical manner. --- RC3_type Morphological type from RC3 number=7 Bytes 37-43 (RC3_type) The alphanumeric morphological type from the RC3. --- Mark 3 1st Han-Mould data file RC3num Number in computer-readable RC3 file number=1 See Note (1) for a82file1.dat. --- UGCnum Number in computer-readable UGC file number=1 See Note (1) for a82file1.dat. --- ESOnum Number in computer-readable ESO file number=1 See Note (1) for a82file1.dat. --- PGCnum Principal Galaxy Catalog number --- Catnum Unique number in Mark 3 HM catalog number=2 Catnum is a record number uniquely assigned to each Han-Mould galaxy in the Mark III analysis. The data for HM galaxies come from four different papers: Catnum 1 to 209: Han, M.-S. 1992, ApJS 81, 35. 210 to 316: Mould, J. et al. 1993, ApJ 409, 14 317 to 373: Mould, J. et al. 1991, ApJ 383, 467. 374 to 429: Han, M.-S and Mould, J 1992, ApJ 396, 453. (Perseus-Pisces sample) 430 to 433: Field galaxies found in these surveys Of these galaxies, six are not given distance predictions for various reasons: Catnum Name 186 E576-32 399 U1344 430 Z180059 431 N3989 432 N3987 433 N3993 There are also six galaxies observed twice, once by Han 1992, again by Han and Mould 1992. Both sets of observations are included in the distance file: Catnum1 Catnum2 Name 3 414 N444 4 415 N452 5 417 N536 16 408 U841 17 409 U987 19 412 U1066 Separately, the 48 galaxies towards the Great Attractor region observed by Bothun et al. (ApJ 388, 253) are not included in this survey for a combination of two reasons: a) Only 48 galaxies in the sample and b) almost complete overlap with better calibrated samples (e.g. 33 galaxies in common with Mathewson et al.). --- Name Name assigned by HM number=3 Name: The naming convention for galaxies follows the convention: A = Anonymous, RA (hr,min), Dec (deg) in usual convention N = NGC I = IC U = UGC E = ESO number, but with or without preceding E in front of number Z, C = Zwicky, field+number --- RAhr 1950 Right Ascension, in decimal hours number=4 Coordinates are expressed in decimal numbers. RA is in hour, declination in degrees. To convert RA to standard hr,min,sec, one must successively convert the decimal part of this number to min and sec. Similarly for declination. h DEdeg 1950 Declination, in decimal degrees number=4 Coordinates are expressed in decimal numbers. RA is in hour, declination in degrees. To convert RA to standard hr,min,sec, one must successively convert the decimal part of this number to min and sec. Similarly for declination. deg GLON Galactic longitude deg GLAT Galactic latitude deg HelioV Heliocentric radial velocity number=5 HelioV is the heliocentric radial velocity of the galaxy as quoted from the HM papers. CMB_V is the radial velocity of the galaxy relative to the Cosmic Microwave Background, using the COBE heliocentric-to-CMB correction of 368.6 km/sec towards l=264.7deg, b=48.2deg. km/s CMB_V Radial velocity w.r.t. CMB number=5 HelioV is the heliocentric radial velocity of the galaxy as quoted from the HM papers. CMB_V is the radial velocity of the galaxy relative to the Cosmic Microwave Background, using the COBE heliocentric-to-CMB correction of 368.6 km/sec towards l=264.7deg, b=48.2deg. km/s Inclin Inclination of galaxy as quoted by HM deg Log(a/b) Log of axial ratio, obs by HM --- Extinc_I Galactic Extinction in I-band number=6 Burstein-Heiles reddenings E(B-V), converted to I-band extinctions by the relation A_I = 1.68(E(B-V)). mag HM_Imag Galaxy total I mag, as observed number=7 HM_Imag is the I band magnitude for the galaxy, as observed. For Catnum values 1 to 209, this magnitude is within the 23.5 mag/arcsecsq surface brightness isophote. For Catnum values 210 to 433, this magnitude is within the 24 mag/arcsecsq isophote level. HM_Imagc is the corrected total magnitude obtained by subtracting the correction Extinc_I (bytes 96-99) only from HM_Imag. mag HM_Imagc HM_Imag corrected for Extinc_I only number=7 HM_Imag is the I band magnitude for the galaxy, as observed. For Catnum values 1 to 209, this magnitude is within the 23.5 mag/arcsecsq surface brightness isophote. For Catnum values 210 to 433, this magnitude is within the 24 mag/arcsecsq isophote level. HM_Imagc is the corrected total magnitude obtained by subtracting the correction Extinc_I (bytes 96-99) only from HM_Imag. mag Mark 3 2nd Han-Mould data file Catnum Unique number in Mark 3 HM catalog number=1 See note (2) for hmfile1.dat --- CMB_V Radial velocity w.r.t. CMB number=2 Bytes 7-12 (CMB_V) is the radial velocity of the galaxy relative to the Cosmic Microwave Background, using the COBE heliocentric-to-CMB correction of 368.6 km/sec towards l=264.7deg, b=48.2deg. km/s DelV_cor 21 cm Delta(V), inclination-corrected number=3 Bytes 15-17 (DelV_cor) is the HI velocity width profile, corrected for internal velocity dispersion as given in the Han, Mould et al. paper. Bytes 20-22 (DelV_obs) is the HI velocity width profile, as observed. Bytes 79-83 (LgDelVHM) is the logarithm of DelV_cor. km/s DelV_obs 21 cm Delta(V), as observed number=3 Bytes 15-17 (DelV_cor) is the HI velocity width profile, corrected for internal velocity dispersion as given in the Han, Mould et al. paper. Bytes 20-22 (DelV_obs) is the HI velocity width profile, as observed. Bytes 79-83 (LgDelVHM) is the logarithm of DelV_cor. km/s Extinc_B Galactic extinction, B-band number=4 Bytes 25-28 (Extinc_B) are values of 4E(B-V), with E(B-V) using the Burstein-Heiles method as quoted in the RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). If galaxy not in RC3, E(B-V) taken from either UGC or ESO computer catalogs of Burstein having Burstein-Heiles reddenings, or calculated directly from the Burstein-Heiles computer-readable reddening maps. mag Bc_RC3 =-9.99 Extinc-corr B_T mag from RC3 number=5 Bytes 30-34 (B_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 37-40 (LogD_RC3) and 43-46 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. mag LogD_RC3 Log D_25 from RC3 number=5 Bytes 30-34 (B_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 37-40 (LogD_RC3) and 43-46 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. .1arcmin RC3_axis =-0.99 Log (a/b) from RC3 number=5 Bytes 30-34 (B_RC3) is the Extinc_B-corrected RC3-quoted B_T magnitude or, if unavailable, the Extinc_B-corrected Harvard magnitude m_B. Note that this magnitude is only corrected for Galactic extinction. Bytes 37-40 (LogD_RC3) and 43-46 (RC3_axis) are the values of the B-band Log D_25 (as observed) and log (a/b) from the RC3. --- D-MajESO ESO eye-determ B band major axis number=6 Bytes 49-52 (D_MajESO) and 55-58 (D_Min_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 61-64 (B_magELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 67-70 (R_magELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 73-76 (D_MajELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). arcmin D-MinESO ESO eye-determ B band minor axis number=6 Bytes 49-52 (D_MajESO) and 55-58 (D_Min_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 61-64 (B_magELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 67-70 (R_magELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 73-76 (D_MajELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). arcmin B-magELV ESO-LV B-band magnitude number=6 Bytes 49-52 (D_MajESO) and 55-58 (D_Min_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 61-64 (B_magELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 67-70 (R_magELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 73-76 (D_MajELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). mag R-magELV ESO-LV R-band magnitude number=6 Bytes 49-52 (D_MajESO) and 55-58 (D_Min_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 61-64 (B_magELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 67-70 (R_magELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 73-76 (D_MajELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). mag D-MajELV ESO-LV B band major axis diameter number=6 Bytes 49-52 (D_MajESO) and 55-58 (D_Min_ESO) are the blue band eye-measured B-band major axis and minor axis of the Galaxy as quoted in Lauberts (1982). Bytes 61-64 (B_magELV) is the B-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 67-70 (R_magELV) is the R-band total magnitude of the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). Bytes 73-76 (D_MajELV) is the B-band major axis diameter for the galaxy taken from the Lauberts-Valentijn Surface Photometry ESO Catalog (1989). arcmin LgDelVHM Log of DelV_cor number=3 Bytes 15-17 (DelV_cor) is the HI velocity width profile, corrected for internal velocity dispersion as given in the Han, Mould et al. paper. Bytes 20-22 (DelV_obs) is the HI velocity width profile, as observed. Bytes 79-83 (LgDelVHM) is the logarithm of DelV_cor. km/s Name Han, Mould et al. Name for Galaxy number=7 Name: The naming convention for galaxies follows the convention: A = Anonymous, RA (hr,min), Dec (deg) in usual convention N = NGC I = IC U = UGC E = ESO number, but with or without preceding E in front of number Z, C = Zwicky, field+number --- Mark 3 3rd Han-Mould data file Catnum Unique number in Mark 3 HM catalog number=1 See Note (2) for hmfile1.dat --- B-I_cat1 =-9.99 B_RC3 minus I_HM, extinc-corr number=2 These parameters are galaxy colors determined by taking catalog values of magnitudes and the Mathewson et al. I band magnitude. These values are corrected for Galactic extinction only (i.e., no inclination correction has been applied). Bytes 7-11 (B-I_cat1) is the B-I total magnitude using RC3 B_T and I_HM. Bytes 13-17 (B-I_cat2) is the B-I total magnitude using ESO-LV B_T and I_HM. Bytes 19-23 (R-I_cat1) is the R-I total magnitude using ESO-LV R_T and I_HM. RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). ESO catalog (Lauberts 1982). ESO-LV catalog - Surface Photometry Catalog of the ESO galaxies (Lauberts and Valentijn 1989). mag B-I_cat2 =-9.99 B_ESO-LV minus I_HM, extinc-corr number=2 These parameters are galaxy colors determined by taking catalog values of magnitudes and the Mathewson et al. I band magnitude. These values are corrected for Galactic extinction only (i.e., no inclination correction has been applied). Bytes 7-11 (B-I_cat1) is the B-I total magnitude using RC3 B_T and I_HM. Bytes 13-17 (B-I_cat2) is the B-I total magnitude using ESO-LV B_T and I_HM. Bytes 19-23 (R-I_cat1) is the R-I total magnitude using ESO-LV R_T and I_HM. RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). ESO catalog (Lauberts 1982). ESO-LV catalog - Surface Photometry Catalog of the ESO galaxies (Lauberts and Valentijn 1989). mag R-I_cat2 =-9.99 R_ESO-LV minus I_HM, extinc-corr number=2 These parameters are galaxy colors determined by taking catalog values of magnitudes and the Mathewson et al. I band magnitude. These values are corrected for Galactic extinction only (i.e., no inclination correction has been applied). Bytes 7-11 (B-I_cat1) is the B-I total magnitude using RC3 B_T and I_HM. Bytes 13-17 (B-I_cat2) is the B-I total magnitude using ESO-LV B_T and I_HM. Bytes 19-23 (R-I_cat1) is the R-I total magnitude using ESO-LV R_T and I_HM. RC3 (de Vaucouleurs et al. 1991, as electronically distributed by Harold Corwin [rc39.all version]). ESO catalog (Lauberts 1982). ESO-LV catalog - Surface Photometry Catalog of the ESO galaxies (Lauberts and Valentijn 1989). mag Lg(a/b)E Log (a/b), ESO eye measures number=3 Bytes 26-29 (Lg(a/b)E) is the log (a/b) of the galaxy as determined from the ESO catalog. Bytes 32-35 ((a/b)ELV) is the log (a/b) of the galaxy as determined from the ESO-LV catalog. --- (a/b)ELV Log (a/b), ESO-LV measures number=3 Bytes 26-29 (Lg(a/b)E) is the log (a/b) of the galaxy as determined from the ESO catalog. Bytes 32-35 ((a/b)ELV) is the log (a/b) of the galaxy as determined from the ESO-LV catalog. --- D-a/b1 Log(a/b)RC3 minus Log(a/b)HM number=4 These are differences between the various measures of axial ratios for each galaxy. Bytes 37-41 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_HM. Bytes 43-47 (D-a/b2) is the difference, log(a/b)_ESO minus Log(a/b)_HM. Bytes 49-53 (D-a/b3) is the difference, log(a/b)_ESO-LV minus Log(a/b)_HM. Bytes 55-59 (D-a/b4) is the difference, log(a/b)_UGC minus Log(a/b)_HM. --- D-a/b2 Log(a/b)ESO minus Log(a/b)HM number=4 These are differences between the various measures of axial ratios for each galaxy. Bytes 37-41 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_HM. Bytes 43-47 (D-a/b2) is the difference, log(a/b)_ESO minus Log(a/b)_HM. Bytes 49-53 (D-a/b3) is the difference, log(a/b)_ESO-LV minus Log(a/b)_HM. Bytes 55-59 (D-a/b4) is the difference, log(a/b)_UGC minus Log(a/b)_HM. --- D-a/b3 Log(a/b)ESO-LV minus Log(a/b)HM number=4 These are differences between the various measures of axial ratios for each galaxy. Bytes 37-41 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_HM. Bytes 43-47 (D-a/b2) is the difference, log(a/b)_ESO minus Log(a/b)_HM. Bytes 49-53 (D-a/b3) is the difference, log(a/b)_ESO-LV minus Log(a/b)_HM. Bytes 55-59 (D-a/b4) is the difference, log(a/b)_UGC minus Log(a/b)_HM. --- D-a/b4 Log(a/b)UGC minus Log(a/b)HM number=4 These are differences between the various measures of axial ratios for each galaxy. Bytes 37-41 (D-a/b1) is the difference, log(a/b)_RC3 minus Log(a/b)_HM. Bytes 43-47 (D-a/b2) is the difference, log(a/b)_ESO minus Log(a/b)_HM. Bytes 49-53 (D-a/b3) is the difference, log(a/b)_ESO-LV minus Log(a/b)_HM. Bytes 55-59 (D-a/b4) is the difference, log(a/b)_UGC minus Log(a/b)_HM. --- f_DB_type1 Indication of peculiar RC3_type number=5 Byte 61 (f_type) This parameter is 1 if the Hubble type given in the RC3 includes the parameter P in such a way that the galaxy is identified as being peculiar, an S0 or an S0/a. The parameter is zero otherwise. --- f_Incl_3 HM inclination quality 1 number=6 Byte 63 (q_Incl_3) This parameter tests for consistency between the axial ratio of the galaxy as given by the RC3 and that given by HM. If the value in Bytes 43-47 (D-a/b1) is 0.30 or greater, this means strong disagreement in axial ratio measurements, and this parameter is one. Otherwise, this parameter is zero. --- DB_type1 Burstein numerical morph type from RC3 number=7 See Note (9) for matfile3.dat --- DB_type2 Burstein numerical morph type, UGC or ESO number=7 See Note (9) for matfile3.dat --- RC3_type Morphological type from RC3 number=8 Bytes 73-79 (RC3_type) and bytes 81-89 (oth_type) These are the alphanumeric galaxy morphological types as given by both the RC3 and by the other catalog (either ESO or UGC) in which the galaxy is found. Either RC3_type or oth_type is blank if no morphological class is given. --- oth_type Morphological type from ESO or UGC number=8 Bytes 73-79 (RC3_type) and bytes 81-89 (oth_type) These are the alphanumeric galaxy morphological types as given by both the RC3 and by the other catalog (either ESO or UGC) in which the galaxy is found. Either RC3_type or oth_type is blank if no morphological class is given. --- HM cluster (HMCL) ind dist file W91 cluster (W91CL) ind dist file W91 Per-Pis (W91PP) ind dist file Courteau-Faber (CF) ind dist file Mathewson etal (MAT) ind dist file Aaronson etal (A82) ind dist file Catnum Unique number in Mark 3 Sample catalog number=1 Bytes 1-4 (Catnum) is a record number uniquely assigned to each galaxy in each data sample. Use this number to correspond the data in this file to the basic data files (i.e., ...filex.lst) for this galaxy sample. Bytes 6-10 (PGCnum) is the number of the galaxy in the Principal Galaxy Catalog (Paturel et al. 1991). --- PGCnum Principal Galaxy Catalog number number=1 Bytes 1-4 (Catnum) is a record number uniquely assigned to each galaxy in each data sample. Use this number to correspond the data in this file to the basic data files (i.e., ...filex.lst) for this galaxy sample. Bytes 6-10 (PGCnum) is the number of the galaxy in the Principal Galaxy Catalog (Paturel et al. 1991). --- Name Galaxy Name number=2 N = NGC (first name preference) I = IC (2nd preference) U = UGC (Nilson 1973) (3rd preference) E = ESO (Lauberts 1982) (3rd preference) Z = Zwicky, field+number (4th preference) A = Anonymous, RA (hr,min), Dec (deg) (4th preference) --- Gp_code =-1 Potent Group number code number=3 Bytes 21-23 (Gp_code) is the number of the group assigned to each galaxy. If a galaxy is not assigned to a group, -1 is entered here. All galaxies in the cluster samples (hm and w91cl) are assigned to a group unless they were explicitly excluded from the TF calibration procedure (cf. Willick et al. 1995, ApJ 446, 12). Galaxies in the field samples (w91pp, cf, mat, a82) are placed into groups by the grouping algorithm of Willick et al. (1996, ApJ 457, 460). Group number zero signifies that the algorithm attempted to group the object but could not because it did not have neighbors sufficiently close in redshift space. Group number $-1$ signifies that the object was excluded a priori from the grouping procedure. For example, as explained in Willick et al. 1996 (Sec. 2 of that paper), the grouping algorithm was not applied to objects with ESO diameters smaller than 1.6 arcmin, with eta less than -0.42 or with inclinations less than 35 degrees. In addition, a small number of objects were excluded a priori for what were judged to be unreliable axial ratios. CF galaxies that lie in the Perseus-Pisces region, not otherwise in the w91PP sample, are combined with the w91pp sample for the purpose of forming maximal groups for later velocity analysis. The result is that cf and w91pp group numbers correspond to the same grouped sample. --- GLON Galactic longitude deg GLAT Galactic latitude deg eta Log DelV - 2.5 number=4 Bytes 39-43 (eta = Log DelV - 2.5), where delV is the velocity full width, determined primarily from HI profiles, but in some cases from optical H-alpha rotation curves (cf. Willick et al. 1997). km/s GalMag Corrected Galaxy Magnitude, sample depend number=5 Bytes 45-49 (GalMag) is the galaxy magnitude that goes into the Tully-Fisher distance calculation, fully corrected for Galactic extinction, inclination and redshift/distance dependencies (see Willick et al. 1997 for details). Bytes 56-59 (Mag_corr) is the sum of all the the corrections that are applied to the observed galaxy magnitude to produce GalMag. mag Select Parameter used for galaxy selection number=6 Bytes 51-54 (Select) is the parameter on which the given galaxy sample was initially selected, and it can be either a diameter (in units or arcmin) or a magnitude. The actual diameter parameter can be either the ESO diameter or the UGC diameter. The actual magnitude parameter can be the Zwicky magnitude, or a raw RC3 magnitude (the last applies to a82 data only). This column is meant to signify the quantity that best approximates the sample selection criterion. E.g., for MAT we assume d_eso >= 1.6, for W91PP d_ugc >= 1.0, etc, when putting together "complete" samples. This column is not meant to be "good" data, it's just what the parent catalog gives. --- Mag_corr Corrections from raw to Corrected Mag number=5 Bytes 45-49 (GalMag) is the galaxy magnitude that goes into the Tully-Fisher distance calculation, fully corrected for Galactic extinction, inclination and redshift/distance dependencies (see Willick et al. 1997 for details). Bytes 56-59 (Mag_corr) is the sum of all the the corrections that are applied to the observed galaxy magnitude to produce GalMag. mag A-ext 4(E(B-V))_2, BH method number=7 Bytes 61-64 (A_Ext) Burstein-Heiles (1984, ApJS 54, 33) and unpublished maps) estimated B magnitude extinction, defined as 4.E(B-V). mag Log_a/b Log (axial ratio) use number=8 Bytes 66-70 (Log_a/b) is the log of the axial ratio, major axis divided by minor axis, used for the galaxy in making inclinations corrections to observed maximum rotation velocities, magnitudes and diameters. --- DB_type Burstein morphological code number number=9 Bytes 72-74 (DB_type) is the hierarchical numerical morphological code developed by David Burstein for use with computer-based galaxy catalogs. The system for the RC3, ESO and UGC catalogs follows. Burstein Code Number Classification 10 Ellipticals - normal 11 E - cD or '+' in RC3 12 Compact E's in RC3 14 E? in RC3 15 E-S0 100 S0 101 SB0 110 S0/a 111 SB0/a 120 Sa 121 SBa 122 Sa/SBa 130 Sa/b 131 SBa/b 132 Sa/b/SBa/b 140 Sb 141 SBb 142 Sb/SBb 150 Sb/Sc 151 SBb/c 152 Sb/c/SBb/c 160 Sc 161 SBc 162 Sc/SBc 170 Sc/d 171 SBc/d 172 Sc/d/SBc/d 180 Sd 181 SBd 190 Sd/Irr 191 SBd/Irr 192 SABd/Irr 195 Im 196 IBm 197 IABm 200 Irr 201 Dwarf Irr 210 Irregular labeled 'P' in RC3 (3 galaxies) 300 'S' 305 'SB' 310 'I?','IB?" 350 'L?' 400 Dwarf 500 Compacts 510 N 600 Multiple galaxies 610 Compact groups 620 Clusters 650 Doubles (general) 651 Doubles: E+E, E+S0, S0+S0 652 Doubles: E+S, S0+S 700 Peculiar 900 No galaxy class given If one takes the numerical type and divides by 10 and take the integer result, one gets: Code Number/10 General Classification 1 E and E/S0 10 All S0 11 All S0/a 12 All Sa 13 All Sa/b 14 All Sb 15 All Sb/Sc 16 All Sc 17 All Sc/Sd 18 All Sd 19 All Sd/Irr 20 All Irr 30 All non-divided classified types 40 Dwarf galaxies 50 Compact galaxies and N galaxies 60 Multiple systems 70 Peculiar galaxies 90 No galaxy class given Separately, one can test for SB, and S/SB galaxies by an appropriate manipulation of the code number. In this way, most of the detail in the morphological classification can be used in a numerical manner. In the case of the a82 data set, the morphological code number is that used by the 2nd Reference Catalog of Bright Galaxies (RC2; de Vaucouleurs, de Vaucouleurs & Corwin 1976). --- Dist_tfr Distance, forward TF, raw number=10 Bytes 76-80 (Dist_tfr) is raw forward TF distance, computed using the forward TF parameters given in Willick et al. 1996, sample dependent. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (with errors given): [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 Bytes 82-86 (Dist_tfc) is the forward TF distance, fully corrected for Inhomogeneous Malmquist Bias (IHM) (see Willick et al. 1997). Bytes 88-92 (Dist_tfi) is the raw inverse TF distance, computed using the inverse TF parameters given in Willick et al. 1997, sample dependent: [mat]: eta = -5.96 + 0.1328(M_I) sigma = 0.059 +_0.03 +_0.0016 [w91cl]: eta = -4.23 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [w91pp]: eta = -4.32 + 0.1244(M_r) sigma = 0.049 0.02 0.0031 [cf]: eta = -4.27 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [hm]: eta = -5.58 + 0.1177(M_I) sigma = 0.048 0.03 0.0025 [a82]: eta = -5.98 + 0.0893(M_H) sigma = 0.043 0.04 0.0018 Bytes 112-116 (Dist_iras) is the expected distance derived from the same IRAS reconstruction (beta=0.6) as was used in the Malmquist correction procedure (see Willick et al. 1997, Sec. 5 for details). This distance was computed as the expectation value of true distance, given the observed radial velocity and the IRAS-predicted peculiar velocity and density fields. A small-scale velocity dispersion of 150 km/s was assumed in the calculation. See Strauss \& Willick (1995, Physics Reports, 261, 271; Sec. 8.1.3). Bytes 123-130 (TF_resid) is the residual, in magnitudes, from the group forward Tully-Fisher relation for galaxies defined to be in groups. The value is -9.999 for galaxies not in groups. km/s Dist_tfc Distance, forward TF, IHM-corrected number=10 Bytes 76-80 (Dist_tfr) is raw forward TF distance, computed using the forward TF parameters given in Willick et al. 1996, sample dependent. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (with errors given): [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 Bytes 82-86 (Dist_tfc) is the forward TF distance, fully corrected for Inhomogeneous Malmquist Bias (IHM) (see Willick et al. 1997). Bytes 88-92 (Dist_tfi) is the raw inverse TF distance, computed using the inverse TF parameters given in Willick et al. 1997, sample dependent: [mat]: eta = -5.96 + 0.1328(M_I) sigma = 0.059 +_0.03 +_0.0016 [w91cl]: eta = -4.23 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [w91pp]: eta = -4.32 + 0.1244(M_r) sigma = 0.049 0.02 0.0031 [cf]: eta = -4.27 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [hm]: eta = -5.58 + 0.1177(M_I) sigma = 0.048 0.03 0.0025 [a82]: eta = -5.98 + 0.0893(M_H) sigma = 0.043 0.04 0.0018 Bytes 112-116 (Dist_iras) is the expected distance derived from the same IRAS reconstruction (beta=0.6) as was used in the Malmquist correction procedure (see Willick et al. 1997, Sec. 5 for details). This distance was computed as the expectation value of true distance, given the observed radial velocity and the IRAS-predicted peculiar velocity and density fields. A small-scale velocity dispersion of 150 km/s was assumed in the calculation. See Strauss \& Willick (1995, Physics Reports, 261, 271; Sec. 8.1.3). Bytes 123-130 (TF_resid) is the residual, in magnitudes, from the group forward Tully-Fisher relation for galaxies defined to be in groups. The value is -9.999 for galaxies not in groups. km/s Dist_tfi Distance, inverse TF, raw number=10 Bytes 76-80 (Dist_tfr) is raw forward TF distance, computed using the forward TF parameters given in Willick et al. 1996, sample dependent. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (with errors given): [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 Bytes 82-86 (Dist_tfc) is the forward TF distance, fully corrected for Inhomogeneous Malmquist Bias (IHM) (see Willick et al. 1997). Bytes 88-92 (Dist_tfi) is the raw inverse TF distance, computed using the inverse TF parameters given in Willick et al. 1997, sample dependent: [mat]: eta = -5.96 + 0.1328(M_I) sigma = 0.059 +_0.03 +_0.0016 [w91cl]: eta = -4.23 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [w91pp]: eta = -4.32 + 0.1244(M_r) sigma = 0.049 0.02 0.0031 [cf]: eta = -4.27 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [hm]: eta = -5.58 + 0.1177(M_I) sigma = 0.048 0.03 0.0025 [a82]: eta = -5.98 + 0.0893(M_H) sigma = 0.043 0.04 0.0018 Bytes 112-116 (Dist_iras) is the expected distance derived from the same IRAS reconstruction (beta=0.6) as was used in the Malmquist correction procedure (see Willick et al. 1997, Sec. 5 for details). This distance was computed as the expectation value of true distance, given the observed radial velocity and the IRAS-predicted peculiar velocity and density fields. A small-scale velocity dispersion of 150 km/s was assumed in the calculation. See Strauss \& Willick (1995, Physics Reports, 261, 271; Sec. 8.1.3). Bytes 123-130 (TF_resid) is the residual, in magnitudes, from the group forward Tully-Fisher relation for galaxies defined to be in groups. The value is -9.999 for galaxies not in groups. km/s HelioV Heliocentric radial velocity number=11 Bytes 94-98 (HelioV) is the heliocentric radial velocity of the galaxy, as quoted by the original source of data. Bytes 100-104 (Loggp_V) is the radial velocity of the galaxy referred to the Local Group velocity frame via the transformation given by Yahil, Sandage and Tammann (1977, ApJ 217, 903), to be applied to the heliocentric radial velocity: V_corr = -79cos(l)cos(b) + 296sin(l)cos(b) - 36sin(b). Bytes 106-110 (CMB_V) is the radial velocity of the galaxy referred to the Cosmic Microwave Background motion of the Sun. Relative to the heliocentric velocity frame, the CMB motion used is assumed to be 368.6 km/sec towards l = 264.7, b = 48.2. km/s Locgp_V Local Group radial velocity number=11 Bytes 94-98 (HelioV) is the heliocentric radial velocity of the galaxy, as quoted by the original source of data. Bytes 100-104 (Loggp_V) is the radial velocity of the galaxy referred to the Local Group velocity frame via the transformation given by Yahil, Sandage and Tammann (1977, ApJ 217, 903), to be applied to the heliocentric radial velocity: V_corr = -79cos(l)cos(b) + 296sin(l)cos(b) - 36sin(b). Bytes 106-110 (CMB_V) is the radial velocity of the galaxy referred to the Cosmic Microwave Background motion of the Sun. Relative to the heliocentric velocity frame, the CMB motion used is assumed to be 368.6 km/sec towards l = 264.7, b = 48.2. km/s CMB_V Cosmic Microwave Bkgd radial velocity number=11 Bytes 94-98 (HelioV) is the heliocentric radial velocity of the galaxy, as quoted by the original source of data. Bytes 100-104 (Loggp_V) is the radial velocity of the galaxy referred to the Local Group velocity frame via the transformation given by Yahil, Sandage and Tammann (1977, ApJ 217, 903), to be applied to the heliocentric radial velocity: V_corr = -79cos(l)cos(b) + 296sin(l)cos(b) - 36sin(b). Bytes 106-110 (CMB_V) is the radial velocity of the galaxy referred to the Cosmic Microwave Background motion of the Sun. Relative to the heliocentric velocity frame, the CMB motion used is assumed to be 368.6 km/sec towards l = 264.7, b = 48.2. km/s Dist_iras IRAS-predicted distance number=10 Bytes 76-80 (Dist_tfr) is raw forward TF distance, computed using the forward TF parameters given in Willick et al. 1996, sample dependent. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (with errors given): [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 Bytes 82-86 (Dist_tfc) is the forward TF distance, fully corrected for Inhomogeneous Malmquist Bias (IHM) (see Willick et al. 1997). Bytes 88-92 (Dist_tfi) is the raw inverse TF distance, computed using the inverse TF parameters given in Willick et al. 1997, sample dependent: [mat]: eta = -5.96 + 0.1328(M_I) sigma = 0.059 +_0.03 +_0.0016 [w91cl]: eta = -4.23 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [w91pp]: eta = -4.32 + 0.1244(M_r) sigma = 0.049 0.02 0.0031 [cf]: eta = -4.27 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [hm]: eta = -5.58 + 0.1177(M_I) sigma = 0.048 0.03 0.0025 [a82]: eta = -5.98 + 0.0893(M_H) sigma = 0.043 0.04 0.0018 Bytes 112-116 (Dist_iras) is the expected distance derived from the same IRAS reconstruction (beta=0.6) as was used in the Malmquist correction procedure (see Willick et al. 1997, Sec. 5 for details). This distance was computed as the expectation value of true distance, given the observed radial velocity and the IRAS-predicted peculiar velocity and density fields. A small-scale velocity dispersion of 150 km/s was assumed in the calculation. See Strauss \& Willick (1995, Physics Reports, 261, 271; Sec. 8.1.3). Bytes 123-130 (TF_resid) is the residual, in magnitudes, from the group forward Tully-Fisher relation for galaxies defined to be in groups. The value is -9.999 for galaxies not in groups. km/s Dens_over Local galaxy over-density number=12 Bytes 118-123 (Dens_over) is the local galaxy overdensity defined as (n_g-n_0)/n_0 where n_g is the local number density of galaxies and n_0 the mean number density, obtained from the IRAS reconstruction of the galaxy density field. The IRAS density was evaluated at the IHM-corrected forward TF distance when Locgp_V is less than 1000 km/s; otherwise it is calculated at the the IRAS-expected distance. --- TF_resid =-9.999 Tully-Fisher resid, groups only number=10 Bytes 76-80 (Dist_tfr) is raw forward TF distance, computed using the forward TF parameters given in Willick et al. 1996, sample dependent. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (with errors given): [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 Bytes 82-86 (Dist_tfc) is the forward TF distance, fully corrected for Inhomogeneous Malmquist Bias (IHM) (see Willick et al. 1997). Bytes 88-92 (Dist_tfi) is the raw inverse TF distance, computed using the inverse TF parameters given in Willick et al. 1997, sample dependent: [mat]: eta = -5.96 + 0.1328(M_I) sigma = 0.059 +_0.03 +_0.0016 [w91cl]: eta = -4.23 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [w91pp]: eta = -4.32 + 0.1244(M_r) sigma = 0.049 0.02 0.0031 [cf]: eta = -4.27 + 0.1190(M_r) sigma = 0.047 0.02 0.0032 [hm]: eta = -5.58 + 0.1177(M_I) sigma = 0.048 0.03 0.0025 [a82]: eta = -5.98 + 0.0893(M_H) sigma = 0.043 0.04 0.0018 Bytes 112-116 (Dist_iras) is the expected distance derived from the same IRAS reconstruction (beta=0.6) as was used in the Malmquist correction procedure (see Willick et al. 1997, Sec. 5 for details). This distance was computed as the expectation value of true distance, given the observed radial velocity and the IRAS-predicted peculiar velocity and density fields. A small-scale velocity dispersion of 150 km/s was assumed in the calculation. See Strauss \& Willick (1995, Physics Reports, 261, 271; Sec. 8.1.3). Bytes 123-130 (TF_resid) is the residual, in magnitudes, from the group forward Tully-Fisher relation for galaxies defined to be in groups. The value is -9.999 for galaxies not in groups. mag HM cluster (HMCL) gp dist file W91 cluster (W91CL) gp dist file CF+W91 merged (WCF) gp dist file Mathewson etal (MAT) gp dist file Aaronson etal (A82) gp dist file W91 PP (W91PP) gp dist file HM+W91 merged (HMW) gp dist Gp_code Unique Group number in Mark 3 catalog number=1 Bytes 1-3 (Gp_code) is a record number uniquely assigned to each galaxy group within a given data sample. Each galaxy in the Independent Distance files is given a Gp_code if it is placed into a group. Bytes 4-6 (num_gal) is the number of galaxies in this group. In corresponding the galaxies in the Independent Distance files to the groups in these files, num_gal acts as a checksum on group identification. IMPORTANT: Groups are, in general, defined separately for each data sample. In most cases no attempt was made to place galaxies from different samples into the same group, with two exceptions: In the file mark3_hmw_g, the ten clusters common to the W91CL and HMCL samples have been merged and the distances suitably averaged. However, the group numbers in the HMCL and W91CL singles files correspond to hmcl_g and w91cl_g, not to wcf_g. In the file mark3_wcf_g, 23 CF galaxies in the PP region, but not present in the W91PP sample, were grouped along with the 326 W91PP galaxies. The W91PP and CF singles files have group numbers that correspond to WCF. See Willick et al. (1997) for further details. --- num_gal Number of galaxies in group number=1 Bytes 1-3 (Gp_code) is a record number uniquely assigned to each galaxy group within a given data sample. Each galaxy in the Independent Distance files is given a Gp_code if it is placed into a group. Bytes 4-6 (num_gal) is the number of galaxies in this group. In corresponding the galaxies in the Independent Distance files to the groups in these files, num_gal acts as a checksum on group identification. IMPORTANT: Groups are, in general, defined separately for each data sample. In most cases no attempt was made to place galaxies from different samples into the same group, with two exceptions: In the file mark3_hmw_g, the ten clusters common to the W91CL and HMCL samples have been merged and the distances suitably averaged. However, the group numbers in the HMCL and W91CL singles files correspond to hmcl_g and w91cl_g, not to wcf_g. In the file mark3_wcf_g, 23 CF galaxies in the PP region, but not present in the W91PP sample, were grouped along with the 326 W91PP galaxies. The W91PP and CF singles files have group numbers that correspond to WCF. See Willick et al. (1997) for further details. --- GLON Mean Galactic longitude of group deg GLAT Mean Galactic latitude of group deg mean_eta Mean of (Log DelV - 2.5) for group number=2 Bytes 22-27 (mean_eta) is the mean value, <eta> = <Log DelV - 2.5> for all the spiral galaxies of this particular sample in the group. km/s tf_scatt Scatter in TF relation for group number=3 Bytes 29-32 (tf_scatt) is the observed scatter about the TF relation for the galaxies in this group. This estimate is corrected for selection bias and degrees of freedom (i.e., it is not just rms residual, because the group distance modulus is a free parameter in the fit; cf. Willick etal. 1996, 1997). mag Dist_tfc Forward TF distances for group number=4 Bytes 34-38 (Dist_tfc) and Bytes 40-44 (Dist_tfi) are the distances estimated for the group according to either a forward TF distance relation (tfc) or an inverse TF distance relation (tfi). Both are corrected for selection bias (however, this bias is small for tfi). See Willick etal. (1996, 1997) for details. The W91PP group file included for completeness only; WCF is suggested for velocity analysis. The HMW group file contains only the 10 clusters common to HMCL and W91CL (cf. Willick et al. 1995). These distances are used by the POTENT algorithm for these clusters. km/s Dist_tfi Inverse TF distance for group number=4 Bytes 34-38 (Dist_tfc) and Bytes 40-44 (Dist_tfi) are the distances estimated for the group according to either a forward TF distance relation (tfc) or an inverse TF distance relation (tfi). Both are corrected for selection bias (however, this bias is small for tfi). See Willick etal. (1996, 1997) for details. The W91PP group file included for completeness only; WCF is suggested for velocity analysis. The HMW group file contains only the 10 clusters common to HMCL and W91CL (cf. Willick et al. 1995). These distances are used by the POTENT algorithm for these clusters. km/s e_Dist* Group distance modulus error number=5 Bytes 46-49 (e_dist) is the Distance Modulus uncertainty for the group, estimated from taking the observed scatter in the TF relation for ALL galaxies in this sample (sigtf) and dividing by the square root of num_gal. The values of sigtf assigned to each data set is as follows: Data Sample sigtf mark3_gp_hmcl 0.40 mag mark3_gp_hmpp 0.40 mark3_gp_w91cl 0.38 mark3_gp_w91pp 0.38 mark3_gp_cf 0.38 mark3_gp_mat 0.43 mark3_gp_a82 0.47 mag HelioV Mean Heliocentric radial velocity number=6 Bytes 51-55 (HelioV) is the heliocentric radial velocity of the galaxy, as quoted by the original source of data. Bytes 57-61 (Loggp_V) is the radial velocity of the galaxy referred to the Local Group velocity frame via the transformation given by Yahil, Sandage and Tammann (1977, ApJ 217, 903), to be applied to the heliocentric radial velocity: V_corr = -79cos(l)cos(b) + 296sin(l)cos(b) - 36sin(b). Bytes 63-67 (CMB_V) is the radial velocity of the galaxy referred to the Cosmic Microwave Background motion of the Sun. Relative to the heliocentric velocity frame, the CMB motion is assumed to be 368.6 km/sec towards l = 264.7, b = 48.2. km/s Locgp_V Local Group radial velocity for grp number=6 Bytes 51-55 (HelioV) is the heliocentric radial velocity of the galaxy, as quoted by the original source of data. Bytes 57-61 (Loggp_V) is the radial velocity of the galaxy referred to the Local Group velocity frame via the transformation given by Yahil, Sandage and Tammann (1977, ApJ 217, 903), to be applied to the heliocentric radial velocity: V_corr = -79cos(l)cos(b) + 296sin(l)cos(b) - 36sin(b). Bytes 63-67 (CMB_V) is the radial velocity of the galaxy referred to the Cosmic Microwave Background motion of the Sun. Relative to the heliocentric velocity frame, the CMB motion is assumed to be 368.6 km/sec towards l = 264.7, b = 48.2. km/s CMB_V Cosmic Microwave Bkgd radial vel, grp number=6 Bytes 51-55 (HelioV) is the heliocentric radial velocity of the galaxy, as quoted by the original source of data. Bytes 57-61 (Loggp_V) is the radial velocity of the galaxy referred to the Local Group velocity frame via the transformation given by Yahil, Sandage and Tammann (1977, ApJ 217, 903), to be applied to the heliocentric radial velocity: V_corr = -79cos(l)cos(b) + 296sin(l)cos(b) - 36sin(b). Bytes 63-67 (CMB_V) is the radial velocity of the galaxy referred to the Cosmic Microwave Background motion of the Sun. Relative to the heliocentric velocity frame, the CMB motion is assumed to be 368.6 km/sec towards l = 264.7, b = 48.2. km/s Name Name of Cluster for certain files number=7 Bytes 69-77 (Name) is the cluster name for the w91cl and hmcl samples. For the remaining samples, this entry is blank. Five HMPP clusters have been included in the HMCL sample. These five clusters (#s 32-36 in the hmcl file) were NOT included in the Paper I TF calibration. However, it was found that their inclusion in the calibration procedure has a negligible effect on the TF calibration parameters. Distances and scatter resulting from the calibration algorithm with them included are given here. No effort to modify them for the tiny differences between the Paper I/II TF calibration and the calibration that results with their inclusion was necessary. --- Matched Spiral galaxy distances PGCnum Principal Galaxy Catalog number number=1 Bytes 1-5 (PGCnum) is the number of the galaxy in the Principal Galaxy Catalog (Paturel et al. 1991). --- HelioV Heliocentric radial velocity number=2 Bytes 24-28 (HelioV) is the mean heliocentric radial velocity of the galaxy, averaged from the quoted values of the data samples being matched for this galaxy. (Note: in the table that appears in Willick et al. (1997), the Galactic longitude and latitude of these objects are indicated prior to the radial velocity. The Galactic coordinates are also included in the version of this table on the Web site maintained by Willick.) km/s eta_hm Log DelV - 2.5 for HM data number=3 Bytes 16-21 (eta_hm), Bytes 35-40 (eta_w91c), Bytes 54-59 (eta_w91p), Bytes 73-78 (eta_cf), Bytes 92-97 (eta_mat), Bytes 111-116 (eta_a82): This is the quoted values of Log DelV - 2.5 for the galaxy for the given data sample. km/s GMag_hm Galaxy Magnitude, HM data number=4 Bytes 23-27 (GMag_hm), Bytes 42-46 (GMag_w91c), Bytes 61-65 (GMag_w91p), Bytes 80-84 (GMag_cf), Bytes 99-103 (GMag_mat), Bytes 118-122 (GMag_a82): This the quoted galaxy magnitude for the given data sample. mag dist_hm Forward raw TF distance for HM data number=5 Bytes 29-33 (dist_hm), Bytes 48-52 (dist_w91c), Bytes 67-71 (dist_w91p), Bytes 86-90 (dist_cf), Bytes 105-109 (dist_mat), Bytes 124-128 (dist_a82): This is the quoted "raw" forward TF distance, computed using the forward By "raw" we mean these distances are NOT corrected for Malmquist bias or selection bias. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (cf. Willick et al. 1996c), with errors given. [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 km/s eta_w91c Log DelV - 2.5 for W91CL data number=3 Bytes 16-21 (eta_hm), Bytes 35-40 (eta_w91c), Bytes 54-59 (eta_w91p), Bytes 73-78 (eta_cf), Bytes 92-97 (eta_mat), Bytes 111-116 (eta_a82): This is the quoted values of Log DelV - 2.5 for the galaxy for the given data sample. km/s GMag_w91c Galaxy Magnitude, W91CL data number=4 Bytes 23-27 (GMag_hm), Bytes 42-46 (GMag_w91c), Bytes 61-65 (GMag_w91p), Bytes 80-84 (GMag_cf), Bytes 99-103 (GMag_mat), Bytes 118-122 (GMag_a82): This the quoted galaxy magnitude for the given data sample. mag dist_w91c Forward raw TF dist for W91CL data number=5 Bytes 29-33 (dist_hm), Bytes 48-52 (dist_w91c), Bytes 67-71 (dist_w91p), Bytes 86-90 (dist_cf), Bytes 105-109 (dist_mat), Bytes 124-128 (dist_a82): This is the quoted "raw" forward TF distance, computed using the forward By "raw" we mean these distances are NOT corrected for Malmquist bias or selection bias. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (cf. Willick et al. 1996c), with errors given. [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 km/s eta_w91p Log DelV - 2.5 for W91PP data number=3 Bytes 16-21 (eta_hm), Bytes 35-40 (eta_w91c), Bytes 54-59 (eta_w91p), Bytes 73-78 (eta_cf), Bytes 92-97 (eta_mat), Bytes 111-116 (eta_a82): This is the quoted values of Log DelV - 2.5 for the galaxy for the given data sample. km/s GMag_w91p Galaxy Magnitude, W91PP data number=4 Bytes 23-27 (GMag_hm), Bytes 42-46 (GMag_w91c), Bytes 61-65 (GMag_w91p), Bytes 80-84 (GMag_cf), Bytes 99-103 (GMag_mat), Bytes 118-122 (GMag_a82): This the quoted galaxy magnitude for the given data sample. mag dist_w91p Forward raw TF dist for W91PP data number=5 Bytes 29-33 (dist_hm), Bytes 48-52 (dist_w91c), Bytes 67-71 (dist_w91p), Bytes 86-90 (dist_cf), Bytes 105-109 (dist_mat), Bytes 124-128 (dist_a82): This is the quoted "raw" forward TF distance, computed using the forward By "raw" we mean these distances are NOT corrected for Malmquist bias or selection bias. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (cf. Willick et al. 1996c), with errors given. [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 km/s eta_cf Log DelV - 2.5 for CF data number=3 Bytes 16-21 (eta_hm), Bytes 35-40 (eta_w91c), Bytes 54-59 (eta_w91p), Bytes 73-78 (eta_cf), Bytes 92-97 (eta_mat), Bytes 111-116 (eta_a82): This is the quoted values of Log DelV - 2.5 for the galaxy for the given data sample. km/s GMag_cf Galaxy Magnitude, CF data number=4 Bytes 23-27 (GMag_hm), Bytes 42-46 (GMag_w91c), Bytes 61-65 (GMag_w91p), Bytes 80-84 (GMag_cf), Bytes 99-103 (GMag_mat), Bytes 118-122 (GMag_a82): This the quoted galaxy magnitude for the given data sample. mag dist_cf Forward raw TF distance for CF data number=5 Bytes 29-33 (dist_hm), Bytes 48-52 (dist_w91c), Bytes 67-71 (dist_w91p), Bytes 86-90 (dist_cf), Bytes 105-109 (dist_mat), Bytes 124-128 (dist_a82): This is the quoted "raw" forward TF distance, computed using the forward By "raw" we mean these distances are NOT corrected for Malmquist bias or selection bias. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (cf. Willick et al. 1996c), with errors given. [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 km/s eta_mat Log DelV - 2.5 for MAT data number=3 Bytes 16-21 (eta_hm), Bytes 35-40 (eta_w91c), Bytes 54-59 (eta_w91p), Bytes 73-78 (eta_cf), Bytes 92-97 (eta_mat), Bytes 111-116 (eta_a82): This is the quoted values of Log DelV - 2.5 for the galaxy for the given data sample. km/s GMag_mat Galaxy Magnitude, MAT data number=4 Bytes 23-27 (GMag_hm), Bytes 42-46 (GMag_w91c), Bytes 61-65 (GMag_w91p), Bytes 80-84 (GMag_cf), Bytes 99-103 (GMag_mat), Bytes 118-122 (GMag_a82): This the quoted galaxy magnitude for the given data sample. mag dist_mat Forward raw TF distance for MAT data number=5 Bytes 29-33 (dist_hm), Bytes 48-52 (dist_w91c), Bytes 67-71 (dist_w91p), Bytes 86-90 (dist_cf), Bytes 105-109 (dist_mat), Bytes 124-128 (dist_a82): This is the quoted "raw" forward TF distance, computed using the forward By "raw" we mean these distances are NOT corrected for Malmquist bias or selection bias. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (cf. Willick et al. 1996c), with errors given. [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 km/s eta_a82 Log DelV - 2.5 for A82 data number=3 Bytes 16-21 (eta_hm), Bytes 35-40 (eta_w91c), Bytes 54-59 (eta_w91p), Bytes 73-78 (eta_cf), Bytes 92-97 (eta_mat), Bytes 111-116 (eta_a82): This is the quoted values of Log DelV - 2.5 for the galaxy for the given data sample. km/s GMag_a82 Galaxy Magnitude, A82 data number=4 Bytes 23-27 (GMag_hm), Bytes 42-46 (GMag_w91c), Bytes 61-65 (GMag_w91p), Bytes 80-84 (GMag_cf), Bytes 99-103 (GMag_mat), Bytes 118-122 (GMag_a82): This the quoted galaxy magnitude for the given data sample. mag dist_a82 Forward raw TF distance for A82 data number=5 Bytes 29-33 (dist_hm), Bytes 48-52 (dist_w91c), Bytes 67-71 (dist_w91p), Bytes 86-90 (dist_cf), Bytes 105-109 (dist_mat), Bytes 124-128 (dist_a82): This is the quoted "raw" forward TF distance, computed using the forward By "raw" we mean these distances are NOT corrected for Malmquist bias or selection bias. The Forward TF relations use for each data sample, and the passband for the quoted GMag are as follows (cf. Willick et al. 1996c), with errors given. [mat] (I-band): M = -5.79 + 6.80(eta) sigma = 0.43 +_0.03 +_0.08 [w91cl] (r-band): M = -4.18 + 7.73(eta) sigma = 0.38 0.02 0.21 [w91pp] (r-band): M = -4.28 + 7.12(eta) sigma = 0.38 0.02 0.18 [cf] (r-band): M = -4.22 + 7.73(eta) sigma = 0.38 0.02 0.21 [hm] (I-band): M = -5.48 + 7.87(eta) sigma = 0.40 0.03 0.16 [a82] (H-band): M = -5.95 + 10.29(eta) sigma = 0.47 0.04 0.22 km/s Mark 3 E galaxy data_1 file GINnum Galaxy identification number number=1 GINnum is the number uniquely assigned each galaxy for catalog work. The value of the number corresponds to the source of data: 1-577 comes from the 7 Samurai survey. 581-655 comes from Lucey & Carter. 660-795 comes from the Dressler-Faber data. 800-872 are galaxies for which the Log_sig and/or Log_D_n values are taken from more than one source (listed by code as data_src; see Note (11)). There are many more galaxies in this file than in egalf2.dat owing to the fact that many galaxies do not have any, or complete, distance related data. --- Name Galaxy name number=2 The name of the galaxy as given by the original data source: A = Abell cluster number and galaxy number; e.g. AXXXX-YYY Ab = Abell cluster number plus letter designation for galaxy, e.g. Ab2199I Anon = Anonymous galaxy designation, e.g. Anon1853 or Anon220+42 CR = Chincarini \& Rood (ApJ 1971, 168, 321) number D = Dressler (1980, ApJS 42, 565) number for galaxy E = ESO catalog name, in a format e.g. EXXX-G000 or EXXX-IG000 I = IC number N = NGC number PER = Dressler observations of Perseus galaxies SPS = Dressler (1988, ApJ 329, 519) designation for redshift survey galaxy U = UGC number --- GLON Galactic longitude deg GLAT Galactic latitude deg A-ext_1 4(E(B-V)), Burstein-Heiles method number=3 4 x E(B-V) taken from Burstein \& Heiles (1982 ApJS 54, 33) and computerized reddening maps. mag GPnum Group/Cluster assignment number number=4 GPnum is the number given to the group or cluster to which the galaxy has been assigned. See Faber et al. (1989) for details. In general GPnum values of 0 are single galaxies (118 galaxies); GPnum between 20 and 110, and 274, 275 and 279 are galaxies in groups with more than one member in this data set (370 galaxies); GPnum between 200 and 299, not otherwise cited are galaxies known to be in a group or cluster, but for which we only have one galaxy measured (56 galaxies). --- HelioVI Heliocentric radial velocity of galaxy number=5 HelioVI is the heliocentric radial velocity of the individual galaxy, as given by the data source(s). When a galaxy has been measured more than once, the value given in an average of the sources. HelioVG is the heliocentric radial velocity of the group in which the the galaxy is contained. This heliocentric velocity is the average of all known galaxies in that group/cluster, not just those in the Egal sample. km/s HelioVG Heliocentric radial velocity of group number=5 HelioVI is the heliocentric radial velocity of the individual galaxy, as given by the data source(s). When a galaxy has been measured more than once, the value given in an average of the sources. HelioVG is the heliocentric radial velocity of the group in which the the galaxy is contained. This heliocentric velocity is the average of all known galaxies in that group/cluster, not just those in the Egal sample. km/s (B-V)_0 Reddening-corrected B-V color number=6 Photoelectric B-V color for the galaxy within a 67 arcsec diameter aperture, as given by Burstein et al. (1987, ApJS 64, 601). mag B-T Total B magnitude number=7 B_T, log_A_e, SB_e and Log D_n are the photometric parameters derived either from photoelectric aperture growth curves (Burstein et al. 1987), or CCD images (Burstein et al. 1987; Lucey & Carter 1989; Dressler & Faber 1990). All are either observed in, or transformed to, the B mag passband. log A_e is the effective circular aperture for the galaxy (the circular aperture containing 1/2 the galaxy light); SB_e is the effective circular mean surface brightness. D_n is the diameter within which the galaxy has a mean B mag surface brightness of 20.75 mag/arcsec^2. mag Log_A_e Effective diameter number=7 B_T, log_A_e, SB_e and Log D_n are the photometric parameters derived either from photoelectric aperture growth curves (Burstein et al. 1987), or CCD images (Burstein et al. 1987; Lucey & Carter 1989; Dressler & Faber 1990). All are either observed in, or transformed to, the B mag passband. log A_e is the effective circular aperture for the galaxy (the circular aperture containing 1/2 the galaxy light); SB_e is the effective circular mean surface brightness. D_n is the diameter within which the galaxy has a mean B mag surface brightness of 20.75 mag/arcsec^2. .1arcmin q_A_e quality parameter for Log_A_e number=8 Quality parameters for the quoted values. See Burstein et al. (1987) for the meaning of these parameters. q = 0, 3 or 4 for a parameter means it is bad and not to be used for serious work. --- q_D_n quality parameter for Log_D_n number=8 Quality parameters for the quoted values. See Burstein et al. (1987) for the meaning of these parameters. q = 0, 3 or 4 for a parameter means it is bad and not to be used for serious work. --- q_B_T quality parameter for B_T number=8 Quality parameters for the quoted values. See Burstein et al. (1987) for the meaning of these parameters. q = 0, 3 or 4 for a parameter means it is bad and not to be used for serious work. --- SB_e Mean effect. B mag surf brightness number=7 B_T, log_A_e, SB_e and Log D_n are the photometric parameters derived either from photoelectric aperture growth curves (Burstein et al. 1987), or CCD images (Burstein et al. 1987; Lucey & Carter 1989; Dressler & Faber 1990). All are either observed in, or transformed to, the B mag passband. log A_e is the effective circular aperture for the galaxy (the circular aperture containing 1/2 the galaxy light); SB_e is the effective circular mean surface brightness. D_n is the diameter within which the galaxy has a mean B mag surface brightness of 20.75 mag/arcsec^2. mag/arcsec Log_sig Log (velocity dispersion) number=9 Log_10 of velocity dispersion, in km/s, as quoted by the source(s). If more than one source of velocity dispersion, the values are averaged. Velocity dispersion used is the one corrected for distance-aperture effect (see Davies et al. ApJS 64, 581). km/s Log_D_n Log D_n parameter (0.1 arcmin) number=7 B_T, log_A_e, SB_e and Log D_n are the photometric parameters derived either from photoelectric aperture growth curves (Burstein et al. 1987), or CCD images (Burstein et al. 1987; Lucey & Carter 1989; Dressler & Faber 1990). All are either observed in, or transformed to, the B mag passband. log A_e is the effective circular aperture for the galaxy (the circular aperture containing 1/2 the galaxy light); SB_e is the effective circular mean surface brightness. D_n is the diameter within which the galaxy has a mean B mag surface brightness of 20.75 mag/arcsec^2. .1arcmin Mg_2 Mg_2 line index number=10 The absorption line index Mg_2 for the galaxies, as quoted by the source(s). If more than one source, the values are averaged. Mg_2 values have been aperture-corrected as given in Davies et al. (1987). mag data_src Source of data number=11 Data Sources: 1 = 7 Samurai (Faber et al., Burstein et al., Davies et al.) 2 = Dressler & Faber 3 = Lucey and Carter Combinations can be 12 (7S+DF), 13 (7S+LC); 23 (DF+LC) and 123 (all three). --- RAh 1950 Right Ascension, hours of time h RAm 1950 Right Ascension, minutes of time min RAs 1950 Right Ascension, seconds of time s DE- Dec sign --- DEd 1950 Declination, degrees deg DEm 1950 Declination, arcmin arcmin DEs 1950 Declination, arcsec arcsec Mark 3 E galaxy data_2 file GINnum Galaxy identification number number=1 GINnum is the number uniquely assigned each galaxy for catalog work. The value of the number corresponds to the source of data: 1-577 comes from the 7 Samurai survey. 581-655 comes from Lucey & Carter. 660-795 comes from the Dressler-Faber data. 800-872 are galaxies for which the Log_sig and/or Log_D_n values are taken from more than one source (see egalf1.dat or the sources). --- GPnum Group/Cluster assignment number number=2 GPnum is the number given to the group or cluster to which the galaxy has been assigned. See Faber et al. (1989) for details. In general GPnum values of 0 are single galaxies (118 galaxies); GPnum between 20 and 110, and 274, 275 and 279 are galaxies in groups with more than one member in this data set (370 galaxies); GPnum between 200 and 299, not otherwise cited are galaxies known to be in a group or cluster, but for which we only have one galaxy measured (56 galaxies). --- HelioV Heliocentric radial velocity number=3 HelioV is the heliocentric radial velocity of the galaxy, as given by the data sources. When a galaxy has been measured more than once, the value given in an average of the sources. km/s LocGpV Local Group radial velocity number=4 LocGpV is the Local Group radial velocity of the galaxy, given by the general prescription used in the Mark 2 catalog: km/s PecV1 Peculiar velocity, smooth Malmquist bias number=5 PecV1 is the predicted peculiar velocity assuming a smooth Malmquist bias correction, and referred to the velocity of the galaxy with respect to the Cosmic Microwave Background. DistMB1 is the smooth Malmquist bias-corrected distance, in units of km/s. To get the CMB velocity used here, simply add PecV1 to DistMB1. Distraw is the predicted distance of the galaxy or group WITHOUT any Malmquist bias correction added. To get the peculiar velocity predicted without a Malmquist bias, simply take the difference between DistMB1 and Distraw and add this to PecV1. Note: The peculiar velocities listed here are revised from the original Mark II values, owing to a downward correction of predicted distance by a factor of 0.965, to bring E galaxy distances into accord with spiral galaxy distances. Hence, both DistMB1 and Distraw are 0.965 the value in the original Mark II, and PecV1 is the difference between the CMB velocity and the new value of DistMB1. km/s DistMB1 Smooth Malmquist bias-corrected distance number=5 PecV1 is the predicted peculiar velocity assuming a smooth Malmquist bias correction, and referred to the velocity of the galaxy with respect to the Cosmic Microwave Background. DistMB1 is the smooth Malmquist bias-corrected distance, in units of km/s. To get the CMB velocity used here, simply add PecV1 to DistMB1. Distraw is the predicted distance of the galaxy or group WITHOUT any Malmquist bias correction added. To get the peculiar velocity predicted without a Malmquist bias, simply take the difference between DistMB1 and Distraw and add this to PecV1. Note: The peculiar velocities listed here are revised from the original Mark II values, owing to a downward correction of predicted distance by a factor of 0.965, to bring E galaxy distances into accord with spiral galaxy distances. Hence, both DistMB1 and Distraw are 0.965 the value in the original Mark II, and PecV1 is the difference between the CMB velocity and the new value of DistMB1. km/s Distraw Raw distance number=5 PecV1 is the predicted peculiar velocity assuming a smooth Malmquist bias correction, and referred to the velocity of the galaxy with respect to the Cosmic Microwave Background. DistMB1 is the smooth Malmquist bias-corrected distance, in units of km/s. To get the CMB velocity used here, simply add PecV1 to DistMB1. Distraw is the predicted distance of the galaxy or group WITHOUT any Malmquist bias correction added. To get the peculiar velocity predicted without a Malmquist bias, simply take the difference between DistMB1 and Distraw and add this to PecV1. Note: The peculiar velocities listed here are revised from the original Mark II values, owing to a downward correction of predicted distance by a factor of 0.965, to bring E galaxy distances into accord with spiral galaxy distances. Hence, both DistMB1 and Distraw are 0.965 the value in the original Mark II, and PecV1 is the difference between the CMB velocity and the new value of DistMB1. km/s GLON Galactic longitude deg GLAT Galactic latitude deg Log_sig Log (velocity dispersion) number=6 Log_10 of velocity dispersion, in km/s, as quoted by the source(s). If more than one source of velocity dispersion, the values are averaged. Velocity dispersion used is the one corrected for distance-aperture effect (see Davies et al. ApJS 64, 581). km/s Log_D_n Log D_n parameter (0.1 arcmin units) number=7 D_n is the diameter within which the galaxy has a mean B mag surface brightness of 20.75 mag/arcsec^2. Given in log units of 0.1 arcmin. .1arcmin J.A. Willick & D. Burstein Stanford/ASU 1996 Aug 21 The Astronomical Data Center thanks Dr. Burstein for not only providing these data but also responding extensively and promptly to our many questions. VII_198.xml A medium-deep survey of a minislice at the north galactic pole. II. The data 7200 VII/200 Minislice at the North Galactic Pole. II. A medium-deep survey of a minislice at the north galactic pole. II. The data C N A Willmer D C Koo N Ellman M J Kurtz A S Szalay Astrophys. J. Suppl. Ser. 104 199 1996 1996ApJS..104..199W A medium-deep survey of a minislice at the north galactic pole. II. The data C N A Willmer D C Koo N Ellman M J Kurtz A S Szalay Astrophys. J. Suppl. Ser. 107 823 1996 1996ApJS..107..823W Galaxies, photometry Galactic pole, north Redshifts cosmology: observations galaxies: distances and redshifts galaxies: photometry surveys A catalogue of 328 positions, redshifts, bJ magnitudes and bJ-rF colours of galaxies down to bJ=20.5 in 4x0.67 degrees slice close to the North Galactic Pole is presented. Two additional tables containing positions, magnitudes, colours and radial velocities for stars and galaxies not in the main catalogue are also included. The photometry errors are about 0.2 for magnitudes and 0.3 for the colours. The radial velocity errors are estimated as being about 70 km/s. The redshift completeness level of the sample is of the order of ~35% at bj=20.
Radial velocities in common with other sources ID Serial number in our main catalog ---- Name Other identification --- RV Radial velocity measured in this work km/s e_RV rms uncertainty on RV km/s RV2 Radial velocity in other measurements km/s e_RV2 rms uncertainty on RV2 km/s r_RV2 Reference of RV2 ZCAT: Huchra 1993, Cat. <VII/193> vH: van Haarlem et al., 1993MNRAS.264...71V Maia: M. Maia, private communication, E94: Ellman 1994, Ph.D. Thesis, Univ. California, Santa Cruz AA: Blumberg & Boksenberg 1995, The Astronomical Almanach for Year 1995 (washington: US Government Printing Office) --- Redshifts, magnitudes and colors for observed galaxies (main table) ID Serial number in full catalogue --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec z Heliocentric redshift --- e_z rms uncertainty on radial velocity km/s n_z Redshift type x = cross-correlation only e = emission lines only c = combined cross-correlation and emission lines --- q_z Redshift quality 1 = Only one feature detected. Discard 2 = Two features detected. Redshift quite likely to be correct 3 = Three features detected. Redshift is correct 4 = Four features recognized. Redshift is correct 5 = Five features recognized. Redshift is correct 6 = Six or more features recognized. Redshift is correct --- bJmag b_J_ magnitude mag bJ-rF b_J_-r_F_ colour index mag PbJmag Percentage estimate of saturated pixels in bJ % PrFmag Percentage estimate of saturated pixels in rF % SB Mean bJ surface brightness mag/arcsec2 Redshifts and magnitudes for observed stars ID Serial number in our main catalog --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec RV Radial velocity km/s e_RV rms uncertainty on RV km/s q_RV Redshift quality identified features in spectrum the quality indicator takes the values: 1 = Only one feature detected. Discard 2 = Two features detected. Redshift quite likely to be correct 3 = Three features detected. Redshift is correct 4 = Four features recognized. Redshift is correct 5 = Five or more features recognized. Redshift is correct --- bJmag b_J_ magnitude mag bJ-rF b_J_-r_F_ colour index mag Redshifts of objects not in the main catalog ID Serial number in catalog derived from PDS scans used in the first observing run. --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec z Heliocentric redshift --- e_z rms uncertainty on radial velocity km/s n_z Redshift type x = cross-correlation only e = emission lines only c = combined cross-correlation and emission lines --- q_z Redshift quality 1 = Only one feature detected. Discard 2 = Two features detected. Redshift quite likely to be correct 3 = Three features detected. Redshift is correct 4 = Four features recognized. Redshift is correct 5 = Five or more features recognized. Redshift is correct --- rFmag Estimated r_F_ magnitude r_F_ magnitude estimated from a fit between the instrumental magnitude measured with the PDS microdensitometer calibrated r_F_ magnitudes. The latter have uncertainties of ~0.20mag. mag C.N.A. Willmer Obs. Nacional J.Marcout, P.Bauer CDS 1997 Jul 07 UNKNOWN UNKNOWN A corrected version, taking into account the Erratum, was kindly supplied by Christopher Willmer (cnaw@dans.on.br) to Nancy G. Roman (roman@adc.gsfc.nasa.gov) and to Heinz J. Andernach (heinz@astro.ugto.mx). Table 2 was added at CDS, in catalogue originally stored as J/ApJS/104/199. VII_200.xml Cross-Identifications in the Abell and Zwicky clusters of galaxies 7201 VII/201 Cross-Identifications in Abell and Zwicky clusters Cross-Identifications in the Abell and Zwicky clusters of galaxies M Kalinkov I Valtchanov I Kuneva Bull. Inf. CDS 49 ??? ??? in press 1998BICDS(in.press) VII/4 : Abell and Zwicky Clusters of Galaxies (Abell+ 1974) Clusters, galaxy Cross identifications A new identification between Abell and Zwicky clusters of galaxies and vice versa is completed. Two convenient files are generated with necessary data for comparing both catalogs; remarks on the cluster matching are also included.
Abell to Zwicky cross-identifications Abell Abell cluster designation --- Cflag 'c' indicates a comment in file azrem.dat 'c' indicates that a comment exists in file azrem.dat 'n' indicates that no Zwicky cluster exists toward the Abell one. --- Field Field where Abell cluster center lies on --- Code Code for correspondence between A- and Z-clusters There are four possibilities: '0' : no matching, '1' : Abell cluster identical with Zwicky cluster, '2' : one Abell cluster is equal to two Zwicky clusters, '+' : two or more Abell clusters are equal to one Zwicky cluster. --- ZCl Zwicky cluster designation --- Rab Abell cluster radius deg Delta Angular distance between Abell and Zwicky clusters centers deg Rz Zwicky cluster radius deg Rabc Abell cluster radius with cosmology deg Znames Up to 10 names (field and consequent number in that field) --- Remarks on azsrt.dat Abell Abell cluster as in file azsrt.dat --- Text Text of comment The codes in comments are with respect to the Abell cluster: 'hb': half background Zwicky or Abell cluster, 'hf': half foreground, 'he': half equidistant, 'f' : foreground, 'b' : background, 'e' : equidistant, 'n' : no Zwicky cluster towards the Abell cluster. --- Zwicky to Abell cross-identifications ZCl Zwicky cluster consequent number --- Cflag indicates a comment in file zarem.dat --- Code Code for correspondence between Z- and A-clusters There are five possibilities: '0' : no matching, '1' : Zwicky cluster identical with Abell cluster, '2' : one Zwicky cluster is equal to two Abell clusters, '3' : one Zwicky cluster is equal to three Abell clusters, '+' : two Zwicky clusters are equal to one Abell cluster. --- Abell Abell cluster designation --- Rz Zwicky cluster radius deg Delta Angular distance between Zwicky and Abell clusters deg Rab Abell cluster radius deg Rabc Abell cluster radius using z deg Znames Up to 12 Zwicky cluster names (field and consequent number in that field) --- Remarks on zasrt.dat ZCl Zwicky cluster as in file azsrt.dat --- Text Text of note several lines of comments may exist for a cluster; the ZCl number if then repeated. The codes in comments are with respect to the Zwicky cluster: 'hb': half background Abell or Zwicky cluster, 'hf': half foreground, 'he': half equidistant, 'f' : foreground, 'b' : background, 'e' : equidistant. --- Francois Ochsenbein CDS 1998 Apr 17 Authors' addresses: M. Kalinkov markal@phys.acad.bg I. Valtchanov ivan@libra.astro.acad.bg Institute of Astronomy, Bulg. Acad. Sci. 72 Tsarigradsko Chausse blvd. BG-1784 Sofia, Bulgaria VII_201.xml A catalog of parameters for globular clusters on the Milky Way 7202 VII/202 Globular Clusters in the Milky Way A catalog of parameters for globular clusters on the Milky Way W E Harris Astron. J. 112 1487 1996, rev. 15 May 1997 1996AJ....112.1487H VII/151 : Structure Parameters of Galactic Globular Clusters (Webbink 1985) http://www.physics.mcmaster.ca/Globular.html : the author's database. Clusters, globular This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog <VII/195>). Important Notice: Please acknowledge the use of this catalog in any published work you derive from it. I would also greatly appreciate receiving any new information, in published or preprint form, which would help me keep the list up to date. William E. Harris <harris@physics.mcmaster.ca> McMaster University
The catalogue of Globular Clusters ID Cluster identification number --- Name Other commonly used cluster name --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Rsun Distance from Sun kpc Rgc Distance from Galactic center, assuming R(Sun)=8.0 kpc kpc X X-component number=1 Position in Sun-centered coordinate system; X points toward Galactic center, Y in direction of Galactic rotation, Z toward North Galactic Pole kpc Y Y-component number=1 Position in Sun-centered coordinate system; X points toward Galactic center, Y in direction of Galactic rotation, Z toward North Galactic Pole kpc Z Z-component number=1 Position in Sun-centered coordinate system; X points toward Galactic center, Y in direction of Galactic rotation, Z toward North Galactic Pole kpc E(B-V) Foreground reddening mag V(HB) V magnitude of the horizontal branch (or RR Lyraes) mag (m-M)V Apparent visual distance modulus mag Vt Integrated V magnitude of the cluster mag MVt Absolute visual magnitude (cluster luminosity) mag (U-B)t Integrated color index number=2 color indices are uncorrected for reddening mag (B-V)t Integrated color index number=2 color indices are uncorrected for reddening mag (V-R)t Integrated color index number=2 color indices are uncorrected for reddening mag (V-I)t Integrated color index number=2 color indices are uncorrected for reddening mag S(RR) Specific frequency of RR Lyr (see Suntzeff et al., 1991ApJ...367..528S) --- HBR Horizontal-branch ratio = (B-R)/(B+V+R) (see Lee, 1990ApJ...363..159L) --- HBt Dickens horizontal-branch morphological type (see Dickens, 1972MNRAS.157..281D) --- [Fe/H] Metallicity in log (base 10) scale Sun SpT Integrated spectral type --- Vr Heliocentric radial velocity km/s e_Vr Observational uncertainty in Vr km/s Vlsr Radial velocity relative to Solar local standard of rest km/s c Central concentration, c = log(Rt/Rc) --- n_c 'c' denotes a core-collapsed cluster --- Rc Core radius arcmin Rh Half-mass radius arcmin u_Rh Uncertainty flag (:) on Rh --- log(Tc) Log (base 10) of core relaxation time yr log(Th) Log (base 10) of relaxation time at the half-mass radius yr muV Central surface brightness in V band mag/arcsec2 log(rhoc) Logarithm of central luminosity density (Solar luminosities per cubic parsec) solLum/pc3 sources.txt Sources and Explanations Francois Ochsenbein CDS 1997 May 14 William E. Harris <harris@physics.mcmaster.ca> UNKNOWN UNKNOWN The catalogue was copied via ftp from www.physics.mcmaster.ca/pub/ VII_202.xml The Las Campanas Redshift Survey 7203 VII/203 Las Campanas Redshift Survey The Las Campanas Redshift Survey S A Shectman S D Landy A Oemler D L Tucker H Lin R P Kirshner P L Schechter Astrophys. J. 470 172 1996 1996ApJ...470..172S http://manaslu.astro.utoronto.ca/~lin/lcrs.html http://www.aip.de:8080/~tucker/lcrs-mirror.html Redshifts Galaxy catalogs QSOs cosmology: observations galaxies: clusters: general galaxies: distances and redshifts surveys In referencing individual galaxies within the LCRS, it is recommended that investigators adhere to the IAU-registered LCRS naming convention, as listed in the online "dictionary of nomenclature of celestial objects" (http://astro.u-strasbg.fr/cgi-bin/Dic), which is: LCRS BHHMMSS.s-DDMMSS, in which the coordinates are equinox 1950.0, RA is truncated (* not rounded *) to a tenth of a second, and DEC is truncated (* not rounded *) to a whole arcsecond. The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700deg^2 in six strips, each 1.5x80deg, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000km/s. Essential features of the galaxy selection and redshift measurement methods are described and tabulated here. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000km/s, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog.
LCRS spectroscopic fields (Table 2) Field Field designation number=1 "W", "E", or "M" means west, east, or middle, --- RA1h First boundary field right ascension (1950.0) h RA1m First boundary field right ascension (1950.0) min RA1s First boundary field right ascension (1950.0) s RA2h Second boundary field right ascension (1950.0) h RA2m Second boundary field right ascension (1950.0) min RA2s Second boundary field right ascension (1950.0) s DE1- First boundary field declination sign --- DE1d First boundary field declination (1950.0) deg DE1m First boundary field declination (1950.0) arcmin DE1s First boundary field declination (1950.0) arcsec DE2- Second boundary field declination sign --- DE2d Second boundary field declination (1950.0) deg DE2m Second boundary field declination (1950.0) arcmin DE2s Second boundary field declination (1950.0) arcsec m1 Lower limit magnitude number=2 Photometric selection limits. Note the catalogs always contain objects outside the photometric limits. Isophotal magnitude m and central magnitude m_c_ of each galaxy must meet the photometric selection criteria m1 <= m < m2 and m_c_ < m_cen_ - 0.5(m2-m) mag m2 Higher limit magnitude number=2 Photometric selection limits. Note the catalogs always contain objects outside the photometric limits. Isophotal magnitude m and central magnitude m_c_ of each galaxy must meet the photometric selection criteria m1 <= m < m2 and m_c_ < m_cen_ - 0.5(m2-m) mag mcen Faint central magnitude limit at m2 number=2 Photometric selection limits. Note the catalogs always contain objects outside the photometric limits. Isophotal magnitude m and central magnitude m_c_ of each galaxy must meet the photometric selection criteria m1 <= m < m2 and m_c_ < m_cen_ - 0.5(m2-m) mag Nfib Designates whether data was obtained with the 50- or 112-object spectrograph system --- Ngal Number of galaxies, within the geometric and photometric limits of the field, which have redshifts. --- f Sampling fraction number=3 Fraction of objects (galaxies plus stars) with velocities, among those objects meeting the photometric selection limits. --- Night Spectroscopic observations date "DD/MM/YY" Frame Spectroscopic exposure number --- plate Spectroscopic plate designation --- Redshift catalog (Table 3) Field Field designation --- p Photometric catalog object number --- mag Isophotal magnitude mag Scan Designation of drift scan used to obtain object photometry --- mc Central magnitude mag RAh Right Ascension (1950.0) h RAm Right Ascension (1950.0) min RAs Right Ascension (may be 60.00) epoch 1950.0 s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (may be 60.0) epoch 1950.0 arcsec s Spectroscopic fiber designation number=1 Columns "s" to "cz55" are blank if not applicable to a particular object --- type Spectrum type (1) number=2 Spectrum type. - c, e, b: galaxy - c: velocity from cross-correlation only - e: velocity from emission-line fitting only - b: velocity from both c and e - *: star - ?: spectrum failed to yield redshift - nh, tc, bl: same as no spectrum attempted (intended spectrum not observed) - QS: QSO - PN: planetary nebula --- cz Heliocentric velocity number=1 Columns "s" to "cz55" are blank if not applicable to a particular object km/s e_cz rms uncertainty on cz km/s sf Product of sampling fraction, apparent magnitude completeness, and central surface brightness completeness factors (1) number=3 See Lin et al. (1996ApJ...464...60L) for more information; sf = f * F * G in the notation of that paper. Objects should be weighted by 1/sf in statistical analyses. Only those galaxies meeting the photometric selection limits have an entry. --- gsf Same as sf but sampling fraction is computed only in a 1000"-radius neighborhood of the galaxy (1) number=4 This attempts to account for any variable geometric sampling effects, e.g. the reduced spectroscopic success at field corners (Shectman et al. 1995, in Wide-Field Spectroscopy and the Distant Universe, proceedings of the 35th Herstmonceux Conference (July 1994), eds. S. J. Maddox & A. Aragon-Salamanca (Singapore: World Scientific), p. 98.). Experience with the galaxy power spectrum (Lin et al., 1996ApJ...471..617L) shows that using gsf instead of sf makes little difference, but it does not hurt to check this for your own analyses. --- cz55 Instrumental constraints prevent two object fibers from approaching closer than 55" on the sky (1) number=5 For an object without a redshift, cz55 is the velocity of its closest neighbor within 55", if one exists, that has a velocity. Only objects within the photometric limits have an entry. To assess the significance of this selection effect for your particular analysis, you can try assigning fake velocities as described in Lin et al. (1996ApJ...471..617L). km/s Patricia Bauer, CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 22-Oct-96 VII_203.xml Galaxy properties at the North Galactic Pole. I. Photometric properties on large spatial scales. 7204 VII/204 Galaxy properties at NGP Galaxy properties at the North Galactic Pole. I. Photometric properties on large spatial scales. S C Odewahn G Aldering Astron. J. 110 2009 1995 1995AJ....110.2009O Galaxy catalogs Magnitudes A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.
All APS-measured galaxies with Omag <= 20.0 (NGP9) No Object number (unique within a plate) --- POSS-I POSS-I plate number (see catalog <VI/25>) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Omag O isophotal magnitude (threshold about 24.5 mag/arcsec2 in B) mag O-E O-E color mag C31 C31 concentration index this index is the ratio between the radius with 75% and 25% of the isophotal light. --- Diam Isophotal (equivalent) diameter arcsec Francois Ochsenbein CDS 1996 Nov 18 UNKNOWN UNKNOWN Copied on 18-Nov-1996 from http://groucho.la.asu.edu/~sco/sco1/data/data.html VII_204.xml Total magnitude, radius, color indices, color gradients and photometric type of galaxies 7206 VII/206 General Photometry of Galaxies Total magnitude, radius, color indices, color gradients and photometric type of galaxies P Prugniel P Heraudeau Astron. Astrophys. Suppl. Ser. 128 299 1998 1998A&AS..128..299P J/A+A/309/749 : Fundamental plane of early type galaxies (Prugniel+ 1996) J/A+AS/127/117 : Kinematics of galaxies (Prugniel+ 1998) J/A+AS/xxx/xxx : Mg2 indices (Golev & Prugniel, 1998) J/AJ/109/517 : Photoelectric types of bright galaxies (Buta+ 1995) VII/155 : RC3 VII/167 : Longo & De Vaucouleurs (1983) http://www-obs.univ-lyon1.fr/~prugniel/cgi-bin/hypercat/ : Hypercat database Galaxy catalogs Galaxies, photometry galaxies: fundamental parameters galaxies: general galaxies: photometry The tables presented here give the catalogue of aperture photometry of galaxies (UBVRI), the associated bibliography, the weight and systematic corrections applied to individual datasets. A table give the results of the growth curve fits; the net of curves adopted is a linear interpolation between the de Vaucouleurs (r^1/4^) and exponential laws. This aperture photometry has three different origins: (i) an update of the catalogue of Buta et al. 1995 (Cat. <J/AJ/109/517>) (ii) published photometric profiles and (iii) aperture photometry performed on CCD images. Fitting growth curves to aperture photometry of galaxies, in UBVRI, we derive (1) the total magnitude, (2) the effective radius, (3) the color indices and (4) gradients and (5) the photometric type of 5066 galaxies. The photometric type is defined to statistically match the revised morphologic type (numerically coded from -6 to +10) and represents the shape of the growth curve. The catalogue is maintained up-to-date in the database HYPERCAT (http://www-obs.univ-lyon1.fr/~prugniel/cgi-bin/hypercat/). This catalogue supersedes the Longo and de Vaucouleurs (1983) catalogue <VII/167>.
Catalogue of aperture photometry Name Galaxy identifier The Name has been adopted by descending the hierarchy: 1) NGC (Cat. <VII/118>) 2) IC (Cat. <VII/118>) 3) UGC (Cat. <VII/26>) or ESO (Cat. <VII/34>) 4) PGC (Cat. <VII/119>) Lyon-Meudon Extragalactic Database internal identifier, also acronimed PGC for numbers greater than 73097. The objects left unfolded into this hierarchy are designated as in the original reference, or by their coordinates: Arrrrrrsdddddd. The galaxy identifiers follow the rule already used in Prugniel & Simien 1996 (J/A+A/309/749) and in Prugniel et al. 1998 (J/A+AS/127/117). --- Type Object type G Galaxy N Not a galaxy (e.g. nebula or cluster) *# foreground star included in the aperture, # is the number of the star M Multiple; the aperture encompasses more than one object --- StarN Number of the star if Type=* --- f_Imag Identification flag U Uncertain identification L Cross identified in leda C Identified by coordinates N Not recognized --- f_Rmag Rejection flag 0 Standard measurement 1 Interactively marqued to be rejected because it departs from the growth curve --- Method Measurement method D Diaphram; Photoelectric photometry S Star count P Simulated aperture photometry from a photometric profile I Aperture measurement on an image --- logA Size of the circular aperture Decimal logarithm of the aperture diameter in 0.1 arcmin [0.1arcmin] Dataset Dataset name detailed in table2.dat --- Vmag Aperture magnitude in V (Johnson) mag u_Vmag Uncertainty on Vmag (: = uncertain) All the uncertainty notes come from original publications --- n_Vmag V color B The magnitude in the V field in B (Johnson) U The magnitude in the V field in U (Johnson) --- B-V B-V (Johnson) mag u_B-V Uncertainty on B-V (: = uncertain) --- n_B-V B-V color U The index in B-V field is U-V (Johnson) --- U-B U-B (Johnson) mag u_U-B Uncertainty on U-B (: = uncertain) --- Rmag R magnitude in the Rsyst system mag u_Rmag Uncertainty on Rmag (: = uncertain) --- n_Rmag Magnitude system The colour system for the R and I bands is coded as: J Johnson C Cousins V Sandage-Visvanathan G Gunn --- Imag I magnitude in the I_syst system mag u_Imag Uncertainty on Imag (: = uncertain) --- n_Imag Magnitude system --- Bibliographic references for table1.dat Dataset Dataset name as in table1.dat and table3.dat --- Bibcode CDS/ADS reference code --- Text Bibliographic reference --- Weights and systematic corrections to be applied to data in table1.dat Dataset Dataset name detailed in table2.dat --- Rres Mean residual in B (unweighted) mag e_Rres rms uncertainty on Rres mag Nmeas Number of measurements used for this reference --- Wres Mean residual in B (after weighting) mag e_Wres rms uncertainty on Wres (after weighting) mag o_Wres weighted number of measurements --- Bcorr Correction on B magnitude Corrected magnitude = (measure in table1.dat) - (correction in table3.dat) mag Vcorr Correction on V magnitude Corrected magnitude = (measure in table1.dat) - (correction in table3.dat) mag Rcorr Correction on R magnitude Corrected magnitude = (measure in table1.dat) - (correction in table3.dat) mag Icorr Correction on I magnitude Corrected magnitude = (measure in table1.dat) - (correction in table3.dat) mag Ucorr Correction on U magnitude Corrected magnitude = (measure in table1.dat) - (correction in table3.dat) mag WG Global weight for this reference --- WZ Zero point weight --- Ngal Number of galaxies observed in this ref. --- WD Density sampling weight --- Derived photometric parameters for the sample's galaxies Name Galaxy identifier The Name has been adopted by descending the hierarchy: 1) NGC (Cat. <VII/118>) 2) IC (Cat. <VII/118>) 3) UGC (Cat. <VII/26>) or ESO (Cat. <VII/34>) 4) PGC (Cat. <VII/119>) Lyon-Meudon Extragalactic Database internal identifier, also acronimed PGC for numbers greater than 73097. The objects left unfolded into this hierarchy are designated as in the original reference, or by their coordinates: Arrrrrrsdddddd. The galaxy identifiers follow the rule already used in Prugniel & Simien 1996 (J/A+A/309/749) and in Prugniel et al. 1998 (J/A+AS/127/117). --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec Bt Asymptotic magnitude in B mag SBe Mean surface brightness within the effective aperture mag/arcsec2 e1 Residual 1-sigma error on Bt mag e2 1-sigma error on log(Ae) log(Ae) is the logarithm of the effective aperture in 0.1 arcmin [0.1arcmin] e3 Effect of e2 on Bt mag e4 1-sigma error on Tphot --- e5 Effect of e4 on Bt mag B-Ve mean B-V within effective aperture mag e_B-Ve 1-sigma error on B-Ve mag gB-V Color gradient in B-V --- U-Be mean U-B within effective aperture mag e_U-Be 1-sigma error on U-Be mag gU-B Color gradient in U-B --- V-Re mean V-R within effective aperture mag e_V-Re 1-sigma error on V-Re mag gV-R Color gradient in V-R --- V-Ie mean V-I within effective aperture mag e_V-Ie 1-sigma error on V-Ie mag gV-I Color gradient in V-I --- Nap Number of aperture available --- LastA log(A)-log(Ae) of the last used Ap [0.1arcmin] Tphot Photometric type --- Mode Mode --- Q Quality flag --- Philippe Prugniel Obs. Lyon 1998 Mar 09 Philippe Prugniel <prugniel@galaxies.univ-lyon1.fr> VII_206.xml Quasars and Active Galactic Nuclei (8th Ed.) 7207 VII/207 Quasars and Active Galactic Nuclei Quasars and Active Galactic Nuclei (8th Ed.) M P Veron-Cetty P Veron ESO Scientific Report 18 ??? ??? 1998 1998ESOSR..18....1V QSOs Active gal. nuclei BL Lac objects This catalogue is an update of the previous versions. It contains 11358 (+2759) quasars (defined as brighter than absolute B magnitude -23), 3334 (+501) AGNs (defined as fainter than absolute B magnitude -23) and 357 (+137) BL Lac objects from 1863 (+201) references.
Quasars (brighter than absolute magnitude -23) Confirmed, probable or possible BL Lac objects Active galaxies (fainter than -23) notRadio '*' if not detected in radio number=1 this flag is blank if the object has been detected as a radio source, and is '*' if not. --- Name Most common name of the object --- RAh Right Ascension J2000 (hours) (see also n_RAh) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec n_RAh Approximative/Optical/Radio position number=2 this flag related to the position takes the values: 'O' for an Optical position with an accuracy better than 1arcsec 'R' for a Radio position with an accuracy better than 1arcsec 'A' for an approximative position --- F6cm 6cm (5GHz) flux Jy r_F6cm Reference of 6cm Flux --- F11cm 11cm (2.7GHz) flux (Jy) Jy r_F11cm Reference of 11cm flux --- l_z limit or method flag on z number=4 n_z may indicate a lower limit on z, or '*', if the redshift is measured by slitless spectroscopy. --- z redshift --- Sp Spectrum classification number=3 the classification of the object is S1: Seyfert 1 spectrum S1h: broad polarized Balmer lines detected S1i: broad Paschen lines observed in the infrared S1n: narrow-line Seyfert 1 S1.0, S1.2, S1.5, S1.8, S1.9: intermediate Seyfert galaxies S2: Seyfert 2 spectrum S3: Seyfert 3 or liner S : unclassified Seyfert S?: possibly a Seyfert H2: nuclear HII region HP: high optical polarization (>3%) BL: confirmed BL Lac object --- n_Vmag '*' for photographic, 'R' for red Vmag --- Vmag magnitude, V or other (see n_Vmag) mag B-V colour index mag U-B colour index mag Mabs Absolute magnitude mag FC Reference of the Finding Chart --- r_Vmag Reference of the Photometry --- r_z Reference of the redshift --- RA1950h Right Ascension B1950 (hours) h RA1950m Right Ascension B1950 (minutes) min RA1950s Right Ascension B1950 (seconds) s DE1950- Declination B1950 (sign) --- DE1950d Declination B1950 (degrees) deg DE1950m Declination B1950 (minutes) arcmin DE1950s Declination B1950 (seconds) arcsec Rejected quasars Name Most common name of the object --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec n_RAh Approximative/Optical/Radio position --- n_z '*' for z measured by slitless spectroscopy --- z Original redshift --- Sp Original classification --- n_Vmag if photographic magnitudes and colours --- Vmag V (or photographic, see n_Vmag) magnitude mag B-V colour index mag U-B colour index mag FC Reference of Finding Chart --- r_Vmag Reference of the Photometry --- r_Sp Reference of Sp --- Sp2 New classification --- r_Sp2 Reference of New classification --- RA1950h Right Ascension B1950 (hours) h RA1950m Right Ascension B1950 (minutes) min RA1950s Right Ascension B1950 (seconds) s DE1950- Declination B1950 (sign) --- DE1950d Declination B1950 (degrees) deg DE1950m Declination B1950 (minutes) arcmin DE1950s Declination B1950 (seconds) arcsec References to tables 1 to 4 RefCode Reference Number number= the text always starts by the "bibcode", a 19-digit code referencing the reference used by SIMBAD, NED, and ADS. When the text cannot fit on a single line, continuation lines are used and the RefCode is repeated, --- Text Text of reference (may be on several lines); the first word is the "bibcode", the text always starts by the "bibcode", a 19-digit code referencing the reference used by SIMBAD, NED, and ADS. When the text cannot fit on a single line, continuation lines are used and the RefCode is repeated, number= the text always starts by the "bibcode", a 19-digit code referencing the reference used by SIMBAD, NED, and ADS. When the text cannot fit on a single line, continuation lines are used and the RefCode is repeated, --- Mira Veron OHP Francois Ochsenbein CDS 1998 Mar 10 Mira Veron <mira@obshpx.obs-hp.fr> UNKNOWN UNKNOWN Previous versions: (1) Veron-Cetty M.P., Veron P., 1984, ESO Scientific Report 1 (2) Veron-Cetty M.P., Veron P., 1985, ESO Scientific Report 4 (3) Veron-Cetty M.P., Veron P., 1987, ESO Scientific Report 5 (Catalogue <VII/93>) (4) Veron-Cetty M.P., Veron P., 1989, ESO Scientific Report 7 (Catalogue <VII/126>) (5) Veron-Cetty M.P., Veron P., 1991, ESO Scientific Report 10 (Catalogue <VII/146>) (6) Veron-Cetty M.P., Veron P., 1993, ESO Scientific Report 13 (Catalogue <VII/166>) (7) Veron-Cetty M.P., Veron P., 1996, ESO Scientific Report 17 (Catalogue <VII/188>) VII_207.xml Faint Galaxies at the North Galactic Pole: The Catalogue 7208 VII/208 Faint Galaxies at the North Galactic Pole Faint Galaxies at the North Galactic Pole: The Catalogue L Infante C J Pritchet G Hertling J. Astron. Data 1, N{deg}2 ??? ??? 1995 1995JAD.....1....2I Galaxy catalogs Galaxies, photometry Galactic pole, north The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&A...282..353), Infante (1994A&AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)
The Catalog of Faint Galaxies at NGP NGPFG Running number --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Jmag Magnitude from IIIaJ plate (blue) mag Fmag Magnitude from IIIaF plate (red) mag Sxx Covariance term number=1 The intensity-weighted covariance terms are defined in the paper; they are related to the size, eccentricity and position angle of the galaxy by: S = sqrt(Sxx + Syy) e = (Syy + sqrt((Sxx-Syy)^2^ + 4 Syx^2^))/(Sxx+Syy) tan(PA) = Sxy/((Sxx + Syy)(1+e)/2 - Syy) arcsec2 Sxy Covariance term number=1 The intensity-weighted covariance terms are defined in the paper; they are related to the size, eccentricity and position angle of the galaxy by: S = sqrt(Sxx + Syy) e = (Syy + sqrt((Sxx-Syy)^2^ + 4 Syx^2^))/(Sxx+Syy) tan(PA) = Sxy/((Sxx + Syy)(1+e)/2 - Syy) arcsec2 Syy Covariance term number=1 The intensity-weighted covariance terms are defined in the paper; they are related to the size, eccentricity and position angle of the galaxy by: S = sqrt(Sxx + Syy) e = (Syy + sqrt((Sxx-Syy)^2^ + 4 Syx^2^))/(Sxx+Syy) tan(PA) = Sxy/((Sxx + Syy)(1+e)/2 - Syy) arcsec2 Peak Height image above sky level mag/arcsec2 Field Area ID --- A1 Areal profile at threshold T+1 number=2 defines the area enclosed by a given isophote. The surface brightness values of the threshold are: ---------------------- Field T(J) T(F) (mag/arcsec2) ---------------------- 1 25.84 24.38 2 25.66 3 25.06 24.60 4 25.79 24.41 5 25.69 24.58 ---------------------- arcsec2 A2 Areal profile at threshold T+2 number=2 defines the area enclosed by a given isophote. The surface brightness values of the threshold are: ---------------------- Field T(J) T(F) (mag/arcsec2) ---------------------- 1 25.84 24.38 2 25.66 3 25.06 24.60 4 25.79 24.41 5 25.69 24.58 ---------------------- arcsec2 A3 Areal profile at threshold T+4 number=2 defines the area enclosed by a given isophote. The surface brightness values of the threshold are: ---------------------- Field T(J) T(F) (mag/arcsec2) ---------------------- 1 25.84 24.38 2 25.66 3 25.06 24.60 4 25.79 24.41 5 25.69 24.58 ---------------------- arcsec2 A4 Areal profile at threshold T+8 number=2 defines the area enclosed by a given isophote. The surface brightness values of the threshold are: ---------------------- Field T(J) T(F) (mag/arcsec2) ---------------------- 1 25.84 24.38 2 25.66 3 25.06 24.60 4 25.79 24.41 5 25.69 24.58 ---------------------- arcsec2 A5 Areal profile at threshold T+16 number=2 defines the area enclosed by a given isophote. The surface brightness values of the threshold are: ---------------------- Field T(J) T(F) (mag/arcsec2) ---------------------- 1 25.84 24.38 2 25.66 3 25.06 24.60 4 25.79 24.41 5 25.69 24.58 ---------------------- arcsec2 A6 Areal profile at threshold T+32 number=2 defines the area enclosed by a given isophote. The surface brightness values of the threshold are: ---------------------- Field T(J) T(F) (mag/arcsec2) ---------------------- 1 25.84 24.38 2 25.66 3 25.06 24.60 4 25.79 24.41 5 25.69 24.58 ---------------------- arcsec2 A7 Areal profile at threshold T+64 number=2 defines the area enclosed by a given isophote. The surface brightness values of the threshold are: ---------------------- Field T(J) T(F) (mag/arcsec2) ---------------------- 1 25.84 24.38 2 25.66 3 25.06 24.60 4 25.79 24.41 5 25.69 24.58 ---------------------- arcsec2 A8 Areal profile at threshold T+128 number=2 defines the area enclosed by a given isophote. The surface brightness values of the threshold are: ---------------------- Field T(J) T(F) (mag/arcsec2) ---------------------- 1 25.84 24.38 2 25.66 3 25.06 24.60 4 25.79 24.41 5 25.69 24.58 ---------------------- arcsec2 Francois Ochsenbein CDS 1998 Apr 16 UNKNOWN UNKNOWN From JAD CD-ROM#1, directory 2 VII_208.xml A search for galaxies behind the Milky Way between l=210deg and 230deg. (Vol. 1) 7209 VII/209 Galaxies Behind the Milky Way A search for galaxies behind the Milky Way between l=210deg and 230deg. (Vol. 1) M Saito H Ohtani A Asonuma N Kashikawa T Maki S Nishida T Watanabe Publ. Astron. Soc. Japan, Vol. 42 603 1990 1990PASJ...42..603S A search for galaxies behind the Milky Way between l=210deg and 230deg. (Vol. 1) M Saito H Ohtani A Baba N Hotta S Kameno S Kurosu K Nakada T Takata Publ. Astron. Soc. Japan, Vol. 43 449 1991 1991PASJ...43..449S A search for galaxies behind the Milky Way between l=210deg and 230deg. (Vol. 1) A T Roman K Nakanishi A Tomita M Saito Publ. Astron. Soc. Jap. 48 679 1996 1996PASJ...48..679R A search for galaxies behind the Milky Way between l=210deg and 230deg. (Vol. 1) A T Roman K Nakanishi M Saito Publ. Astron. Soc. Jap. 50 37-46 1998 1998PASJ...50...37R J/A+AS/104/529 : IRAS galaxies behind the Milky Way (Takata+ 1994) Galaxy catalogs Milky Way galaxies: clusters: general galaxies: general galaxies: redshift galaxies: large galaxies: structure galaxies: Milky Way galaxies: search This catalogue gathers the searches for galaxies of apparent size greater than 0.1mm (6.7") behind the Milky Way from photographic surveys in the near infrared. The four volumes cover the galactic longitude ranges -7 to +43{deg}, and 210 to 250{deg}.
The two catalogs, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito
Volume 1: l=210 to 230 deg Volume 2: l=230 to 250 deg Vol Volume number --- CGMW Running number in volume --- Field Field number of the ESO/SERC Southern Sky Survey --- Xpos X coordinate on the film (1mm ~ 67") mm Ypos Y coordinate on the film (1mm ~ 67") mm RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin GLON Galactic longitude deg GLAT Galactic latitude deg MajDiam Size of apparent major diameter (1mm ~ 67") mm MinDiam Size of apparent minor diameter (1mm ~ 67") mm MType Morphological type class the classes are: E : Elliptical I : Irregular S : Spiral SB : Barred Spiral --- feature Feature of the object the following features are included: Bright, Faint : for surface brightness Asymm, Ring : for morphology Pair, Triple : for close association (If accompanying galaxies are almost in the same position, they are not listed in the catalog). PN+galaxy : a foreground planetary nebula overlaps a galaxy --- CrossId Cross identifications in other catalogs --- Volume 3: l= 8 to 43 deg Vol Volume number --- CGMW Running number in volume --- Plate Name of Schmidt Atlas and field number on which the search was performed --- RefSurv Name of the reference survey the survey are designated by: SR = UK-SR I = UK-I O = POSS I-O EJ = SERC-EJ --- Over1 Field number of overlapping plate --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin GLON Galactic longitude deg GLAT Galactic latitude deg MajDiam Size of apparent major diameter (1mm ~ 67") mm MinDiam Size of apparent minor diameter (1mm ~ 67") mm Feature Feature of the object the following features are included: for the surface brightness: LSB (low) or bright for morphological type: S (spiral), E (elliptical), pec (peculiar) and ND (nuclear dominant) for multiplicity: pair or triplet, which indicates the presence of one galaxy or two galaxies within a few arcminutes. If an accompanying galaxy is nearly at the same position, the companion is not listed in the catalog and is merely indicated as 'pair'. If the object seems to be close to a star or on a star, we denote this as 'near *' or 'with *', respectively. for aspect: If the object is a possible star (the image has circular shape or the faint extended component around a bright star-like object), we denote it as 'star:', where the colon means possible feature. 'PN:' means a possible planetary nebulae, i.e., the image is rather round and the surface brightness distribution seems to be homogeneous or the outer edge of the image is relatively sharp compared with that of a galaxy. --- CrossId Cross identifications in other catalogs --- Volume 4: l= -7 to 16 deg Vol Volume number --- CGMW Running number in volume --- Plate Name of Schmidt Atlas and field number on which the search was performed --- RefSurv Name of the reference survey the survey are designated by: SR = UK-SR R = ESO/SRC-R --- Over1 Field number of overlapping plate --- --- Separator when OVer2 exists --- Over2 Field number of overlapping plate --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg MajDiam Size of apparent major diameter (1mm ~ 67") mm MinDiam Size of apparent minor diameter (1mm ~ 67") mm Feature Feature of the object (see "Note on Feature" section above) --- CrossId Cross identifications in other catalogs --- Patricia Bauer, Francois Ochsenbein CDS 1998 Apr 07 UNKNOWN UNKNOWN * Supersedes VII/140 (Vol. 1 and Vol. 2 only), prepared by ADAC (NAO, Japan) on 22-Apr-1992. * Copied from http://kusastro.kyoto-u.ac.jp/library/deptpub.html on 07-Apr-1998. The files were reformatted at CDS for an homogeneous format of volumes 3 and 4. VII_209.xml A Catalogue of Galactic Supernova Remnants, 1998 September version 7211 VII/211 A Catalogue of Galactic Supernova Remnants A Catalogue of Galactic Supernova Remnants, 1998 September version D A Green Mullard Radio Astronomy Observatory, Cambridge, United Kingdom ??? ??? 1998 1998 VII/187 : the July 1995 version which was superseded by this catalogue VII/210 : the August 1996 version which was superseded by this catalogue http://www.mrao.cam.ac.uk/surveys/snrs/ : the on-line versionGreen, D.A., MNRAS, 209, 449 (1984) =1984MNRAS.209..449G Green, D.A., ApSS, 148, 3, (1988) =1988APSS..148....3G Green, D.A., PASP, 103, 209 (1991) =1991PASP..103..209G Green D.A., 1996, in Supernovae and Supernova Remnants, (the proceedings IAU Colloquium 145), eds McCray R. & Wang Z., (Cambridge University Press), p419. Supernova Remnants Milky Way Nonstellar objects This catalogue of known Galactic supernova remnants (SNRs) is an updated version of the catalogues of Galactic SNRs presented in detail in Green (1984, 1988), in summary form in Green (1991, 1996), and on the World-Wide-Web (versions of July 1995 and August 1996). (Note that version published in Green (1996) was produced in 1993.) This September 1998 version of the catalogue contains 220 SNRs, which is 5 more than listed in the previous version. The basic summary data included in this catalogue for each SNR are its Galactic coordinates, RA and Dec (B1950.0), angular size (in arcmin), type, flux density at 1 GHz, spectral index, and any other names. Notes on these parameters, on possible remnants not included, and questionable SNRs listed in the catalogue are given in full version of the catalogue on the World-Wide-Web. It should be noted that there are serious selection effects which apply to the identification of Galactic SNRs (see Green 1991), so that great care should be taken if these data are used in statistical studies.
Supernova Remnant catalogue GLON Galactic longitude l Galactic Coordinates are the source centroid quoted to the nearest tenth of a degree. (Note: in this catalogue additional leading zeros are not used.) deg GLAT Galactic latitude b deg RAh Right Ascension B1950 hours The accuracy of the quoted values depends on the size of the remnant. For small remnants they are to the nearest few seconds of time and the nearest minute of arc for RA and DEC respectively. For the larger remnants they are rounded to coarser values. They are in every case sufficient to specify a point within the boundary of the remnant. These coordinates are generally deduced from radio maps rather than from X-ray or optical observations, and are B1950.0. h RAm Right Ascension B1950 minutes min RAs Right Ascension B1950 seconds s DE- Declination sign --- DEd Declination B1950 degrees deg DEm Declination B1950 arcminutes arcmin Ang_Size Angular Size of remnant Usually taken from the highest resolution radio map available, although for some barely resolved sources that are thought to be SNRs the only available size is that from Gaussian models after deconvolution with the observed beam size. The boundary of most remnants approximates reasonably well to a circle or an ellipse; a single value is quoted for the angular size of the more nearly circular remnants, which is the diameter of a circle with an area equal to that of the remnant, but for elongated remnants the product of two values is quoted, and these are the major and minor axes of the remnant boundary modeled as an ellipse. In a few cases an ellipse is not a satisfactory description of the boundary of the object (refer to the description of the individual object given the full catalogue entry), although an angular size is still quoted for information. For `filled-centre' remnants the size quoted is for the largest extent of the observed radio emission, not, as at times has been used, the half-width of the centrally brightened peak. arcmin2 type Type of remnant S remnant shows a shell radio structure F remnant shows a filled center ('filled centre') radio structure C remnant shows a composite or combination radio structure S?, C?, F? if there is some uncertainty ? object is conventionally considered a SNR although its nature is poorly known or not well understood. --- l_S(1GHz) Limit flag on S(1GHz) --- S(1GHz) Flux Density at 1 GHz The flux density of the remnant at 1 GHz in Jansky. This is not a measured value, but that deduced from the observed radio frequency spectrum of the source. The frequency of 1 GHz is chosen because flux density measurements at frequencies both above and below this value are usually available. Jy u_S(1GHz) Uncertainty flag on S(1GHz) --- SI Spectral Index of integrated radio emission The spectral index of the integrated radio emission from the remnant is either a value quoted from the literature, or one deduced from the available integrated flux densities of the remnant. For several SNRs a simple spectral model is not adequate to describe their radio emission because the spectral index varies across the face of the remnant or that the integrated spectrum is curved, and in these cases the spectral index includes the 'v' in u_SI. In some cases, for example where the remnant is highly confused with thermal emission, the spectral index is given as '?' since no value can be deduced with any confidence. --- u_SI Uncertainty and variability flag on SI --- alt Other names commonly used Other names commonly used for the object. These are given in parentheses if the remnant is only part of the source. For some objects, notably the Crab Nebula, not all common names are given. --- Dave Green MRAO 1998 Nov 10 UNKNOWN UNKNOWN The on-line version on the World-Wide-Web contains much more information on the individual objects, include many references. VII_211.xml Systematic Properties of Compact Groups of Galaxies 7213 VII/213 Hickson's Compact groups of Galaxies Systematic Properties of Compact Groups of Galaxies P Hickson Astrophys. J. 255 382 1982 1982ApJ...255..382H Systematic Properties of Compact Groups of Galaxies P Hickson Astrophys. J. 259 930 1982 1982ApJ...259..930H Systematic Properties of Compact Groups of Galaxies P Hickson E Kindl J R Auman Astrophys. J. Suppl. Ser. 70 687 1989 1989ApJS...70..687H Systematic Properties of Compact Groups of Galaxies C Mendes de Oliveira P Hickson Astrophys. J. 380 30 1991 1991ApJ...380...30M Systematic Properties of Compact Groups of Galaxies P Hickson C Mendes de Oliveira J P Huchra G G C Palumbo Astrophys. J. 399 353 1992 1992ApJ...399..353H Systematic Properties of Compact Groups of Galaxies C Mendes de Oliveira P Hickson Astrophys. J. 427 684 1994 1994ApJ...427..684M J/A+AS/117/39 : Far-IR properties of Hickson Compact Groups (Allam+, 1996) J/A+A/325/473 : HCG HI-deficiency (Huchtmeier 1997) Clusters, galaxy Galaxies, optical Redshifts Galaxies, photometry Velocity dispersion The catalog of groups (file "groups.dat") is a list of 100 compact groups of galaxies identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2^ and satisfies an isolation criterion. Dynamical parameters were derived for 92 of the 100 groups, which are listed in file "dynamics.dat"; the Hubble constant was assumed to be Ho=100km/s/Mpc. Data about individual galaxies in these groups are merged into the "galaxies.dat" file; these data include photometric parameters, morphology, redshifts and absolute magnitudes originally published in four different papers. They result from CCD observations at CFHT (Canada-France-Hawaii Telescope) in 1983-1985. Redshifts were observed at the 1.5m telescope of the F.L. Whipple Observatory on Mt. Hopkins, Arizona, over the period 1984-1986, in wavelength range 470-710nm; the remaining fainter galaxies were observed with the CFHT.
Catalog of groups (1982 paper, and errata) HCG Number of the group in this catalog --- RAh Right Ascension 1950 hours h RAm Right Ascension minutes min RAs Right Ascension seconds s DE- Declination sign --- DEd Declination degrees (1950) deg DEm Declination arcminutes arcmin DEs Declination arcseconds arcsec Dyna '*' when group has dynamical parameters --- Type Group type Two-character code (a letter followed by a number) classifying the group according to its two brightest members: S The brightest galaxy is a spiral galaxy. E The brightest galaxy is not a spiral galaxy. 1 m(b) - m(a) >= 1.0 2 0.5 <= m(b) - m(a) < 1.0 3 m(b) - m(a) < 0.5 where m(a) and m(b) are the estimated red magnitudes of the brightest and second brightest members, respectively, of the cluster. --- MCount Member count Number of galaxies in the group. Only those galaxies within three magnitudes of the brightest galaxy are counted as members. --- AngSize Angular size Angular diameter, in arcminutes, of the smallest circle containing the geometric centers of all group members. arcmin TotMag Total magnitude of group Total estimated red magnitude of those galaxies counted as group members (see member count, above.) mag Emag Brightest member magnitude Estimated red magnitude of the brightest galaxy in the group, in units of magnitude. mag z Redshift Corrected redshift of the brightest galaxy. In all but ten cases this field is blank; prefer the group redshift supplied in the file "dynamics.dat". --- Aname1 Alternate name 1 Other designations of the group, if any (at most, four). --- Aname2 Alternate name 2 --- Aname3 Alternate name 3 --- Aname4 Alternate name 4 --- Dynamical properties (1992 paper, table3) HCG Group number --- z Group Redshift derived from the median galaxy heliocentric velocity --- n Number of galaxies with accordant velocities --- log(sV) Radial velocity dispersion [km/s] log(V) Estimated instrinsic 3D velocity dispersion [km/s] log(R) Median projected separation [kpc] log(Ho.tc) Crossing time (expressed in 1/Ho units) --- log(Mv) Virial mass of group in log. scale [g] log(Mp) Projected mass [g] log(Ma) Average mass [g] log(Mm) Median mass [g] log(M) Adopted mass [g] log(L) Total blue luminosity of the accordant galaxies [W] log(M/L) Mass-to-light ratio [Sun] log(rho) Mass density [g/cm3] Photometric and Velocity data for galaxies (combined tables from 1989 and 1992 papers) HCG Hickson Group number (groups.dat) --- m_HCG Galaxy in HCG group --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec a Semi-major axis at 25.0mag/arcsec^2^ isophote arcsec b Semi-minor axis at 25.0mag/arcsec^2^ isophote arcsec MType Hubble Morphological type --- T Numeric morphological type the morphological type codes are: --------------------------- Hubble Code RC2 --------------------------- E0-E7 0 -4, -5 S0, SB0 1 -2 S0a, SB0a 2 0 Sa, SBa 3 1 Sab, SBab 4 2 Sb, SBb 5 3 Sbc, SBbc 6 4 Sc, SBc 7 5 Scd, SBcd 8 6 Sd, SBd 9 7 Sdm, SBdm 10 8 Sm, SDm 11 9 Im, IBm 12 10 cI 13 11 --- morph when more morphology in file "morpho.dat" --- RVhel Heliocentric velocity km/s e_RVhel Estimated rms in RVhel km/s q_RVhel Confidence code on RVhel the confidence code is 0 = highest confidence: spectral features clearly visible 1 = lower confidence: spectral features not clearly visible 2 = lowest confidence: very noisy spectra with no obvious features. Only 3 galaxies have q_RVhel=2. --- Bmag B magnitude within 24.5mag/arcsec^2^ isophote mag q_Bmag Confidence level for Bmag confidence levels are: 0 = good 1 = uncertain due to overlapping isophotes 2 = uncertain due to contamination 3 = uncertain due to poor calibration 4 = uncertain due to clouds. (value 5 for HCG 64c unexplained) --- DBmag Diameter of B=24.5mag/arcsec^2^ isophote the diameter is defined as sqrt(Area/{pi}) arcsec Rmag R magnitude within 24.0mag/arcsec^2^ isophote mag q_Rmag Confidence level for Rmag --- DRmag Diameter of R=24.0mag/arcsec^2^ isophote --- B-R Colour within the 24.5mag/arcsec^2^ isophote mag BTmag B_T_ asymptotic magnitude mag BTc B_T_ asymptotic magnitude corrected for internal and external extinction mag e_BTmag Mean error on BTmag mag MB-5log(h) Absolute magnitude of individual galaxies, h=Ho/100, Ho=Hubble constant mag Names Other names --- Morphology (1994 paper, table2) HCG Hickson Group number (groups.dat) --- m_HCG Galaxy in HCG group --- RVhel Heliocentric velocity km/s MType Morphological type --- Comments Comments Abbreviations used in comments: [string 'ansac' in 58a is unexplained] asym. = asymmetric emission = galaxy with emission lines in its nuclear spectrum IR = infrared emitter (Hickson et al. 1989ApJ...341..679H, Sulentic & de Mello Rabaca 1993ApJ...410..520S) morpho = morphology n.c.i. = nonconcentric isophotes r.c. = rotation curve radio = radio-loud galaxies (Menon & Hickson 1985; Menon 1993) tail-like= galaxy has tail-like features vel. = velocity WR = galaxy exhibits Wolf-Rayet spectral features --- Francois Ochsenbein CDS 1999 Jun 07 UNKNOWN UNKNOWN * History of Catalogue VII/85: The catalogue was originally prepared at the Centre de Donnees astronomiques, Strasbourg (CDS), in 1986. It was then received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, in December 1986. The original tape consisted of a single text file containing the catalog data from Table 1 of Systematic Properties of Compact Groups of Galaxies, in a slightly more compact format. ADC personnel deleted eight blank columns from the end of each record in the file to reduce the record size from 80 to 72 bytes and ran a FORTRAN program to check the validity of each field according to its data type and value. Two minor typographic errors discovered in the computer-readable version were then corrected by referring to the published catalog. A possible error was also detected, but not changed, in record number 97, where the DEC seconds field contains a value of 60 (this value appears in the printed version). P. Hickson kindly supplied a list of errata including some corrections in addition to the published erratum. This list is reproduced below; the indicated changes have already been made to the catalog data. ERRATUM HCG AngSize TotMag Emag 14 6.7 12.1 13.0 22 5.0 10.5 11.1 60 2.3 13.4 14.4 69 1.9 12.2 13.1 82 3.1 12.2 13.1 HCG RAh/RAm/RAs DEd/DEm/DEs 03 00 31 39 -07 52 07 31 04 59 08 -04 19 42 74 15 17 14 +21 04 27 89 21 17 34 -04 07 17 * Catalogue VII/213 (F. Ochsenbein, CDS, 07-Jun-1999) This catalogue is a merged version of: - VII/85 (1982ApJ...255..382H), with its ReadMe description made by C.-H. Joseph Lyu [Hughes STX/NASA] on 16-Oct-1995, and of: - 1991ApJ...380...30M (absolute magnitudes) kindly supplied by Claudia Mendes de Oliveira <coliveira@eso.org> in March 1994. - 1989ApJS...70..687H, 1992ApJ...399..353H and 1994ApJ...427..684M kindly supplied by Heinz Andernach; these tables were prepared via OCR and proofread by him in April 1995. VII_213.xml An Optical Catalogue of Radio Galaxies 8003 VIII/3 An Optical Catalogue of Radio Galaxies An Optical Catalogue of Radio Galaxies G Burbidge A H Crowne Astrophys. Journ. Suppl. 40 583 1979 1979ApJS...40..583B Galaxies, radio Redshifts Radio sources Galaxy catalogs This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.
Radio sources identified with optical galaxies RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s piRA Precision indicator of the right ascension Precision indicator of the right ascension; the right ascension is given as HH MM SS.ss with eight possible significant digits. The precision indicator identifies how many of these eight digits are given as blank (i.e. not known) and so may vary between zero and eight. --- DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec piDE Precision indicator of declination Precision indicator of declination: the declination is given as DD MM SS.S with seven possible significant digits. The precision indicator identifies how many of these seven digits are given as blank (i.e. not known) and so may vary between zero and seven. --- refID Reference identification number (file "refs") --- EqPos Code for equatorial position Code for equatorial position: blank = optical position given taken primarily from papers reporting the redshift and identification papers. R = radio position given ("*" in published catalogue). --- FCRnum Finder chart reference number (file "refs") --- OptType Optical type code Optical type code - left justified in field. The type codes and their statistics are given in Table A-2. All types and cluster information (cf. bytes 38-39) is drawn from either the identification reference (cf. bytes 25-27) or the redshift reference (cf. bytes 81-83). --- Rdesc Radio description Radio description which is no longer used. If these bytes are not blank then given object is in a cluster. The radio description codes and their statistics are given in Table A-3. --- V Visual magnitude. Visual magnitude. These values are very uncertain since very few photometric measurements have been made. mag B-V Photoelectric colors if available mag U-B Photoelectric colors if available mag r_V Reference for photometric data (file "refs") --- Z Redshift. Redshift. Most of the redshifts listed are uncorrected for galactic rotation. --- n_Z Redshift (cf. bytes 63-68) qualifier Redshift (cf. bytes 63-68) qualifier: blank - if the value of the redshift (z) is not corrected for galactic rotation. "C" - if z is corrected ("*" in published catalogue) "Q" - if unknown if z has been corrected ("?" in published catalogue). --- LineType Spectral lines type Spectral lines type: "A" - if absorption lines. "E" - if emission lines. "AE"- if absorption and emission. Where no spectral-line lists have been published but mention has been made of the appearance of absorption or emission, it is noted with an "A" or "E" in these bytes. --- CoordID Coordinate designation Coordinate designation given as HHMMSDDX based on equatorial coordinates at epoch B1950.0 where: HH = hours of right ascension MM = minutes of right ascension S = sign of the declination DDX= declination (unit=0.1deg) --- r_Z Redshift (z) reference number (file "refs") --- flux(freq) Radio flux at frequency given in bytes 93-96. Jy freq Frequency in MHz (408 for most entries) MHz r_flux(freq) Reference for radio flux (cf. bytes 85-91) --- SI Radio spectral index between 408 & 1400 MHz Radio spectral index between 408 and 1400 MHz. The spectral index alpha is defined by S(nu) = K. nu**(-alpha) In the published catalogue the symbol ">" following the value of the spectral index indicates a range between 408 and 5000 MHz and the symbol "<" indicates a range between 178 and 408 MHz. No attempt has been made to extrapolate where fluxes have been given at other frequencies (cf. byte 115). --- r_SI Reference for spectral index (file "refs") --- MapRef Primary reference for radio map number --- SIcode Code for spectral index range. Code for spectral index range. This code is for the symbols ">" and "<" as defined above in bytes 102-106. The ">" is coded as an "A" and the "<" is coded as a "B". This byte is blank if other than these two spectral indices. See the file "refs". --- SpNum Number of spectral lines Number of spectral lines used in the computation of the value of the redshift. This number ranges from 0 to 20. --- Lines List of 20 coded spectral lines. List of 20 coded spectral lines. The coded values range from 01 to OR and are defined in Table A-4. The N (cf. bytes 116-117) coded values are at the beginning of this field and the remaining bytes are blank. --- NumRef Number of additional references. --- A-refs Additional references Additional references are five characters each where the first three represent the reference number (file "refs") and the two letter code for the type of reference as follows: ID - identification FC - finder chart Z - redshift S - radio flux (S) SI - radio spectral index (SI) M - radio map --- Alias Other names Other names - maximum of seven names separated by commas with no embedded blanks. Table A-1 gives the codes used in these fields along with their full reference to the published literature --- Seq Sequential counter (range 1-495). --- References in numeric order References in alphabetical order RefNum Reference number Reference number which ranges from 1-414 but only 412 references. --- pchar The period character ("."). --- Ref References References in format usually found in the astronomical literature. --- Francois Ochsenbein CDS C.-H. Joseph Lyu Hughes STX/NASA 1996 Jul 17 The original ADC documentation by Theresa A. Nagy and Robert S. Hill (1981) was used to create this ReadMe file. UNKNOWN UNKNOWN The machine-readable version of the Optical Catalog of Radio Galaxies (Burbidge and Crowne 1979) was received at NASA/Goddard Space Flight Center (NASA/GSFC) from one of the authors (Adelaide Hewitt, formerly A. H. Crowne) in the summer of 1981. Extensive modifications to the format of the machine-readable catalogue have been made. Originally the magnetic tape consisted of card image records on one file which contained the data (five cards per entry) followed by the references. This single file has been divided into two separate files: a data file and a reference file. There are 495 data records and 412 reference records each on a separate file. In addition, the reference file is sorted numerically to generate the three file magnetic tape described herein. The numbers which quantitatively define the precision of the components of the equatorial coordinators have been computed and added to the records to readily identify less precise coordinate availability. Information in byte 24 of the original first data record was moved to byte 28 to add the computed recision indicator for the declination. The coordinate designation, which is the key identifier in the published catalogue, was computed from the given coordinates and added to each record (cf. bytes 73-80) since it was not originally given on the tape for the majority of the records. The number of spectral lines present and the number of additional references have been computed for each record and added (cf. bytes 116-117 and 158-159 respectively in file "refs". One object (#154, 0812-029) had the first of the five data cards missing. The data have been reconstructed from the published catalogue whenever possible. There are several data items that are given in the machine-readable version of the catalogue that are not in the published catalogue and so the values of these were not reconstructed for the missing data record. The radio description (cf. bytes 38-39, file "catalog") is given in the machine-readable version with the note that it is no longer used, but not in the published catalogue. The photometric colors (B-V) and (U-B) are given for very few of the entries in the machine-readable version but also do not appear in the published catalogue. This is also true of the photometric reference for the data values. The frequency (MHz) is another quantity that appears in the digital version of the catalogue but not in the published version. Embedded blanks have been removed from the other names field and commas have been added to separate entries. A sequential counter (range 1 to 495) was added to each data record. The record preceding the references on the original tape contained the number 411 (actually there are 412 references) and was removed. In addition, the last record was a "999" to designate the last card image record was removed. Some references were on a single card image and some continued onto a second card image. The information has been joined together into a single record of equal length for each reference. The counter in the reference file was also inconsistent where some had leading zeros and others did not, and some had the period (".") following the number and others did not. The file that has been produced is consistent in these matters and is defined in file "refs" of this document. Table A-1 is a list of the many designations used in the other names field (cf. bytes 220-269, file "catalog") and the full reference for each. This table was prepared utilizing the information in the published catalogue. Tables A-2 and A-3 respectively represent statistics compiled during the preparation of this document. The statistics are for the counts of coded optical types and radio descriptions respectively. Table A-4 is information originally supplied by the authors and provides the code for spectral lines used in the determination of the redshift (z) value. The user of this catalogue is advised to use the other identifier correspondences available in the published catalogue whose reference is given below. MODIFICATIONS AT CDS (June 1993, F. Ochsenbein): The printed document was used as input for the present documentation. A few misalignments in the file "catalog" have been corrected in records ("Seq") numbers 2, 20, 114, 132, 154, 202, 237, 240, 251, 263 and 428 TABLE A-1: Designations of other names coded plus references to the published source catalogue/list Coded Name Catalogue/List and Reference AO Arecibo Occultation Survey, 430 and 195 MHz. Hazard, C., Gulkis, S., and Bray, A. D. 1967, Ap.J., 148, 669. Hazard, C., Gulkis, S., Sutton, J. 1968, Ap.J., 154, 413. Gulkis, S., Sutton, J., and Hazard, C. 1969, Ap.J., 157, 1047. Lang, K. R., Sutton, J., Hazard, C., and Gulkis, S. 1970, Ap.J., 160, 17. B2 Second Bologna Catalog of Radio Sources, 408 MHz. Colla, G., et al. 1973, Astr. Ap. Suppl., 11, 291. Colla, G., et al. 1970, Astr. Ap. Suppl., 1, 281. Colla, G., et al. 1972, Astr. Ap. Suppl., 7, 1. CTA Caltech Radio Survey, List A, 960 MHz. Harris, D. E., and Roberts, J. A. 1960, Pub. A.S.P., 72, 237. CTD Caltech Radio Survey, List D, 1421 MHz. Kellermann, K. I., and Read, R. B. 1965, Pub. Owens Valley Radio Obs., 1, No. 2,1. DA Dominion Radio Observatory Survey, List A, 1420 MHz. Galt, J. A., and Kennedy, J.E. D. 1968, A.J., 73, 135. DB Dominion Radio Observatory Survey, 10.03 MHz. Bridle, A. H., and Purton, C. R. 1968, A J.,73, 717. DW Dwingeloo-Greenbank Radio Source List, 1417 MHz. Davis, M. M. 1967, Bull. Astr. Inst. Netherlands, 19, 201. GC National Radio Astronomy Observatory 5 GHz Radio Survey. Davis, M. M. 1971, A J., 76, 980. H National Radio Astronomy Observatory Survey, 750 + 1410 MHz. Hoglund,B. 1967,Ap. J.Suppl., 15,61. LHE Long, Haseler, and Elsmore 408 MHz Survey. Long, R. J., Haseler, J. B., and Elsmore, B. 1963, M.N.R.A.S., 125, 313. MC2 Molonglo Radio Catalog, 408 MHz. MC3 Sutton, J. M., Davies, I. M., Little, A. G., and Murdoch, H. S. 1974, Australian J. Phys. Suppl., No. 33, p. 1. Davies, I. M., Little, A. G., and Mills, B. Y. 1973, Australian J. Phys. Suppl., No. 28, p. 1. MSH Mills, Slee, and Hill Radio Survey, 855 MHz. Mills, B. Y., Slee, O. B., and Hill, E. R. Australian J. Phys., 11, 360 (1958) Australian J. Phys., 13, 676 (1960); Australian J. Phys., 14, 497 (1961) NB Mullard Radio Astronomy Observatory Survey, 81.5 MHz. Branson, N. J. B. A. 1967, M.N.R.A.S., 135, 149. NRAO National Radio Astronomy Observatory Catalog, 750 + 1400 MHz Pauliny-Toth, I. I. K., Wade, C. M., and Heeschen, D. S. 1966, Ap. J. Suppl., 13, 65. OA Ohio Source, 1415 MHz. Kraus, J. D., 1964, Nature, 202, 269. Nash, R. T. 1965, A.J., 70, 846. Kraus, J. D., Dixon, R. S., and Fisher, R. O. 1966, Ap. J., 144, 559. OB-OZ Ohio Source, 1415 MHz. Scheer, D. J., and Kraus, J. D. 1967, A.J., 72, 536. Dixon, R. S., and Kraus, J. D. 1968, A.J., 73, 381. Fitch, L. T., Dixon, R. S., and Kraus, J. D. 1969, A J., 74, 612. Ehman, J. R., Dixon, R. S., and Kraus, J. D. 1970, A. J., 75, 351. Brundage, R. K., Dixon, R. S., Ehman, J. R., and Kraus, J. D. 1971, A.J., 76, 777. Ehman, J. R., Dixon, R. S., Ramakrishna, C. M., and Kraus, J. D. 1974, A.J., 79, 144. Rinsland, C. P., Dixon, R. S., Gearhart, M. R., and Kraus, J. D. 1974, A.J., 79, 1129. NOTE: Ohio sources may be found in the catalog by noting that the name is a coordinate designation. The second letter (B-Z, omitting the letter O) gives the hours of right ascension, the first digit gives the declination in 10degrees increments, and the last two digits give the right ascension to 0h01 (thus OQ 172 has 10deg < delta < 20deg and alpha = 14.72h). PKS Parkes Radio Catalog, 408 and 1410 MHz. Staff of CSIRO Division of Radiophysics, ed. J. A. Ekers. 1969, Australian J. Phys. Suppl., No. 7, p. 1. Parkes 2700 MHz Survey. Wall, J. V., Shimmins, A. J., and Merkelijn, J. K. 1971, Australian J. Phys. Suppl., No. 19, p. 1. Shimmins, A. J. 1971, Australian J. Phys. Suppl., No. 21, p.1. Shimmins, A. J., and Bolton, J. G. Australian J. Phys. Suppl., No. 26, p. 1, (1972) J Australian J. Phys. Suppl., No. 32, p. 1. (1974) Bolton, J. G., and Shimmins, A. J. 1973, Australian J. Phys. Suppl., No. 30, p. 1. Bolton, J. G., Shimmins, A. J., and Wall, J. V. 1975, Australian J. Phys. Suppl., No. 34, p. 1. RN Ryle and Neville 178 MHz Survey of Sources North of 86deg. Ryle, M., and Neville, A. C. 1962, M.N.R.A.S., 125, 39. VR Vermilion River Observatory Survey, 610 MHz. MacLeod, J. M., Swenson, G. R,, Jr., Yang, K. S., and Dickel, J. R. 1965, A.J., 70, 756. Wendker, H. J., Dickel, J. R., Yang, K. S., and staff. 1970, A.J., 75, 148. 3C Third Cambridge Radio Catalogue, 159 MHz. Edge, D. O., Shakeshaft, J. R., McAdam, W. B., Baldwin, J. E., and Archer, S. 1959, Mem. R.A.S., 68, 37. 3CR Third Cambridge Radio Catalogue (Revised), 178, MHz. Bennett, A. S.-1962, Mem. R.A.S., 68, 163. NOTE: A few objects listed with a 3C or 3CR number followed by a slash and a second number (as in 3C 93.1/113) are weak sources near strong 3C sources from a survey by Windram, M. D. and Kenderdine,S. 1969, M.N.R.A.S., 146, 265. 4C Fourth Cambridge Radio Catalogue, 178 MHz. Pilkington, J. D. H., and Scott, P. F. 1965, Mem. R.A.S., 69, 183. Gower, J. F. R., Scott, P. F., and Wills, D. 1967, Mem. R.A.S., 71, 49. Caswell, J. L., and Crowther, J. H. 1969, M.N.R.A.S., 145, 181. 4CT A Pencil-Beam Survey of Radio Sources, 178 MHz. Caswell, J. L., and Crowther, J. H. 1969, M.N.R.A.S., 1, 181. 5C Fifth Cambridge Radio Catalogue, 408 MHz. Pooley, G. G., and Kenderdine, S. 1968, M.N.R.A.S., 139, 529. Pooley, G. G. 1969, M.N.R.A.S., 144, 101. Willson, M. A. G. 1970, M.N.R.A.S., 151, 1. TABLE A-2: Statistics of Optical Types. Code Counts Description 174 not given CD 8 CD3 2 CD4 CD5 COM COMP 8 compact D 24 DB 17 DE 2 DEl DE2 2 DE3 5 DE4 2 D2 D3 3 D4 3 D6 D/E3 E 116 ED 8 ED2 3 ED3 2 ED4 2 EO 11 El 2 E2 8 E3 1 E4 2 E5 4 E/CD E/D E/S0 E+DB IRR 1 irregular N 38 N/D PEC 5 peculiar S 4 spiral SA SC 2 SE SEYF 2 Seyfert S0 10 S0P TOTAL 495 TABLE A-3: Statistics of Radio Description Codes. Code Count Description Al 1 Abell 24 A2 1 Abell 115 A3 1 Abell 119 A4 1 Abell 194 A5 1 Abell 262 A6 1 Abell 347 A7 1 Abell 400 A8 1 Abell 407 A9 1 Abell 1367 B0 1 Abell 2251 Bl 1 Abell 1452 B2 1 Abell 1795 B3 1 Abell 2078 B4 1 Abell 2162 B5 1 Abell 2199 B6 1 Abell 2220 B7 3 Abell 2241 B8 1 Abell 2256 B9 1 Abell 2250 Cl 1 Abell 2626 C2 2 Abell 2634 C3 1 Abell 2622 C4 1 Abell 1190 C6 1 Abell 1213 C7 2 C8 1 C9 1 D0 1 Dl 1 D2 1 D3 1 D4 1 D5 1 D6 1 D7 1 D8 1 D9 1 EO 1 C 148 in cluster SG 2 small group G 15 group PR 1 269 not given TOTAL 495 NB. C5 was defined as Abell 779 in the original documentation for this catalogue, but this code was not found for any of the records. However, since the first data card for #154 (coordinate designation 0812-029) was missing, this could account for the discrepancy. This particular galaxy was counted in.the blank code. Since this piece of datum does not appear in the published catalogue there was no way to identify what the radio description code should have been. TABLE A-4: Code for Spectral Lines Used to Determine the Redshift (z). Emission Absorption Code Lambda(A) Line Code Lambda(A) Line 01 3727 [OII] OH 3969 CaII H 02 4959 [OIII] OK 3934 CaII K 03 5007 [OIII] OG 4304 G 04 6584 [NII] OA 5893 NaID (Dl) 05 3869 [NeIII] OB 4861 H-beta 06 4340 HI OC 4340 H-gamma 07 4861 HI OD 3970 H-epsilon 08 6563 HI OE 4102 H-delta 09 6300 [OI] OF 3970 H7 10 3426 [NeV] OJ 5175 MgI 11 3968 [NeIII] OL 5269 MgH 12 4363 [OIII] OM 4384 Fe 13 4686 [HeII] ON 5270 FeI 14 3346 [NeV] OO 4226 CaI 15 5876 [HeI] OP 5162 MgIb 16 4102 H-delta OR 6563 Ha 17 6717 [SII] 18 6731 [SII] 19 3203 HeII 20 3889 H-zeta 21 6548 [NII] 22 3133 OIII 23 --- --- 24 4026 HeI 25 4068 [SII] 26 4076 [SII] 27 5200 [NI] 28 3325 [NeV] 29 3444 [NeV] 30 2799 MgII 31 6725 [SII] 32 6363 [OI] VIII_3.xml The Fourth Cambridge Survey of Radio Sources 8004 VIII/4 Fourth Cambridge Survey of Radio Sources The Fourth Cambridge Survey of Radio Sources J D H Pilkington P F Scott Mem. Roy. Astron. Soc. 69 183 1965 1965MmRAS..69..183P The Fourth Cambridge Survey of Radio Sources J F R Gower P F Scott D Wills Mem. Roy. Astron. Soc. 71 49 1967 1967MmRAS..71...49G Surveys Radio sources The Fourth Cambridge Radio Survey (4C) Catalogue contains all survey data from the papers of Pilkington and Scott (1965) and Gower, Scott and Wills (1967). These data result from a survey of radio sources between declinations -07 and +80 degrees using the large Cambridge interferometer at 178 MHz. The computerized catalog contains for each source the 4C number, 1950 position, measured flux density, accuracy class, galactic coordinates, and remarks. For some sources miscellaneous brief comments such as cross identifications to the 3C catalog or remarks on contamination from nearby sources are given at the ends of the data records. A flag (*) is included if there are additional remarks in the published catalog.
Fourth Cambridge Radio Survey Data ID The 4C number The 4C number. The first byte contains the zone sign; the first two digits give the zone, while the last two sequentially number the source in the zone (there are no sequential numbers over 100). Bytes 7-8 contain the characters ".1" only for source 4C+25.56.1, which was added by Pilkington and Scott (1965) after publication of the catalog. --- RAh Right ascension equinox 1950.0 The positions were determined from interference pattern phases (see Pilkington and Scott 1965). h RAm R.A. in minutes min RAs R.A. in seconds s DE- Sign of declination equinox 1950.0 --- DEd Dec. deg DEm Dec. arcmin FluxDen Flux density (1.0E-26 MKS) at 178 MHz See source references for additional information. Byte 40 is blank for sources having lower accuracy data. W/m2/Hz ErrClas1 Position and flux error class (in number) Numerical code for position and flux density error class. The codes having e's and l's plus *'s are assigned the same numerical codes as those without the asterisks (i.e. be* = be = 21). The codes are as follows: 1 = a 11 = ae 14 = blank 2 = b 21 = be 15 = [1] 3 = c 31 = ce 13 = a* 12 = al 23 = b* 22 = bl 33 = c* 32 = cl [1] a special code indicating that a character class is listed in the published catalog, but the flux density is from 3C only and is enclosed in parentheses. --- GLON Galactic longitude, System II. deg GLAT Galactic latitude, System II. deg ErrClas2 Position & flux error class (character form) Position and flux density error class in character form (lower case letters) corresponding to numerical code in bytes 43-44. The symbols have the following meanings: a,b,c: Error class of source; estimated standard errors for sources in various ranges of flux density are given in Tables II and III of the respective source references. e: Possible right ascension lobe-shift earlier. The magnitude of the lobe shift for each 1 degree interval is given in Tables I of the source references. l: Possible right ascension lobe-shift later. *: The source is confused by a weaker uncataloged one. The weaker source will usually lie within 30' and have a flux density at least 1/3 of the main source. The quoted error class for each source includes the effect of such confusing sources. --- com Remarks Remarks. Only cross identifications to the Revised 3C Catalogue (Bennett 1962) are actually given in the remarks field; however, additional remarks given in the published catalog, for which there is insufficient room in the 8-byte field, are indicated by an asterisk. Asterisks can occur alone or with 3C numbers. --- C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 02 The original ADC documentation by Wayne H. Warren, Jr. (1983) was used to create this ReadMe file. UNKNOWN UNKNOWN The machine-readable version of the 4C catalog was received on magnetic tape from Dr. G. G. Pooley of Mullard Radio Astronomy Observatory, Cambridge on 1 March 1983. As received, the file consisted of 80-byte card images with a blank record following every fifth data record. The following modifications were made so that the data structures conform more closely to those of other computerized catalogs and so that the data are easier to process and to interpret. 1. Blank records, clearly a problem for data processing, searching and sorting, were removed. 2. The 4C numbers in the machine file were written as positive and negative integers (e.g. 7901, -105, -7) rather than as real numbers in the form +/-xx.xx, as they are normally written in the literature. The integers were converted to the present form. 3. Negative declinations had minus signs on both degrees and minutes. The latter were removed, while minus signs were moved to all occur in byte 23 and plus signs were added for positive declinations (previously blank). Signs were also moved or added to byte 55 in the Galactic latitude field. Preceding zeros were added to these fields to make uniform numbers. 4. The file was sorted by 4C number to correspond exactly with the published catalog. The error classes (in character form) and remarks were keyed to a separate data set on disk. After interval checks throughout the then 4843 records, the newly keyed records were added to the original data set. The numerical and character coded classes should be equivalent in all cases. The file was then resorted by 4C number, South to North. 5. There were only 3623 sources in the printed 1967 catalog, while 3624 records are contained in the machine version. Source 4C+48.61, found in the machine catalog, is missing from the published version. The character class for 4C+48.61(a) was obtained from the machine version and inserted. The source 4C+25.56.1, added as an addendum to the 1965 publication, was in the machine version as a duplicate of 4C+25.56. The ".1" was added to the 4C number (bytes 7-8) for this record. 6. The logical record length was changed from 80 bytes to 72 bytes, since bytes 72-80 were never used. 7. Numerical codes for 4C-02.07, 4C+21.19 and 4C+29.58 did not agree with the published catalog, so they were corrected in the machine version. The character and numerical codes have not been checked entirely, so additional disagreements may be found. In these cases, reference should be made to the source papers. 8. Some sources having numerical class code 14 were found to have non-blank character codes in the published catalog. These sources have only 3C flux densities enclosed in parentheses. To distinguish them from published sources with blank class codes, a new numerical code of 15 was defined and added to the appropriate records. VIII_4.xml Catalog of Extragalactic Radio Sources Having Flux Densities Greater Than 1 Jy at 5 GHz 8005 VIII/5 Bright Extragalactic Radio Sources Catalog of Extragalactic Radio Sources Having Flux Densities Greater Than 1 Jy at 5 GHz H Kuehr A Witzel I I K Pauliny-Toth U Nauber Astron. Astrophys. Suppl. 45 367 1981 1981A&AS...45..367K Galaxies, radio Galaxy catalogs Radio sources The catalog is a compilation of 518 extragalactic radio sources with flux densities greater than 1 Jy at 5 GHz. It contains sources from the NRAO-MPI 5-GHz Strong Source Surveys and from re-observation at 5 GHz of sources found in the Parkes 2.7-GHz surveys. All sources were found in 9.811 sr covered by the two surveys. This is essentially the whole sky, excluding the galactic plane (latitudes less than 10 degrees) and the Magellanic Clouds. The catalog includes radio flux densities, radio positions, object classes, visual magnitudes, redshifts, and spectral indices.
Codes for the position references are listed in this document in the appendix. In the main file, errors are given for all radio positions, flux densities, spectral indices, and function coefficients. See the original paper for discussions of the completeness of the catalog, of the compilation of the flux density data, and of the fitting of simple analytic functions to the spectra. The EGRS catalog lists information on 518 objects with one to sixteen flux density values for each source. The file header.dat lists the complete header information for each object. This line has been removed from catalog.dat. There are at most four density values in each record. Records containing fewer than four measurements are filled with blanks on the right. The first word of the file catalog.dat contains the id for the object. refs.dat contains a numerically sorted list of the radio source catalogs cited in the flux density measurement records. For each source catalog the original reference or references (usually one, but in one case as many as three) are listed, as well as the pertinent characteristics of the catalog. When more than one line was needed for a reference up to four continuation lines were used.
Details for each source id Source name The EGRS contains sources from the combined NRAO-MPI 5 GHz Strong Source Survey and Parkes 2.7 GHz Surveys. This is a coordinate-based naming system. --- 3C 3C name If the object was listed in the 3rd Cambridge Radio Catalog (Bennett 1961; 3C), then the full 3C designation is here. If not, then this field is blank. --- RAh Right Ascension (RA) (1950.0) hours h RAm RA (1950.0) minutes min RAs RA (1950.0) seconds s e_RA Error in RA s DE- Declination sign --- DEd Declination (DE) sign deg DEm DE minutes arcmin DEs DE seconds arcsec e_DE Error in DE arcsec pos-ref Position reference The positions listed for the object come either from radio-interferometery measurements (usually) or from the original surveys (occasionally). This two-letter code indicates the source of the coordinates and corresponds to those listed in the Appendix. --- glat Galactic latitude deg cl Object class If the object has been optically identified, this gives the class of the object as a three character code as described in the following. If it has not, this field is blank. QSO = Quasar GAL = Radio galaxy BL = BL Lacertae object EF = Empty field CF = Confused field (i.e., more than one object in the field) --- mag Visual magnitude From Veron and Veron (1979) and Kuehr (1980). mag rshift Redshift km/s ind Spectral index The two point spectral index . . . as determined between 2700 MHz and 5000 MHz. The spectral index is defined here as alpha., where the flux density is assumed proportional to frequency. --- e_ind Sp. I. error --- type Function type For sources with flux density measurements at more than three frequencies, an attempt was made to fit a simple analytic function to the spectrum. This field contains one of four values depending on the result of this fit: LIN = The spectrum was successfully fitted by a straight line of the form y = A + Bx, where x = log v and y = log S Coefficients A and B only will contain data, coefficients C and D will be blank. EXP = The spectrum was fitted by a function of the type y = A + Bx + Cexp(Dx). All four coefficient fields will contain data. CPX = Although there were sufficient data points for the source (i.e., more than three) the spectrum could not be satisfactorily fitted with either of the above functional forms. Such a spectrum was designated complex because it would not be physically meaningful to devise some general analytic form to fit any spectral measurements (i.e. of variable sources whose spectra are generally complex). All coefficient fields will be blank. N<4 = There were data for no more than three frequencies and consequently no fit was attempted. All coefficient fields will be blank. --- A Coefficient A --- e_A A error --- B Coefficient B --- e_B B error --- C Coefficient C --- e_C C error --- D Coefficient D --- Catalog id Source name --- freq-1 Frequency Hz col-1 --- flux-1 Flux density The flux density measurements are listed, in rows, in order of ascending frequency, so that consecutive frequencies run from left to right. The data may be read in ascending frequency order by using a repeating FORTRAN format statement to read successive records. All flux densities given . . . are on the scale of Baars et al. (1977). This scale is based on the absolute radio spectrum of Cassiopeia A. Between 0.3 and 30 GHz it is given by a flux density S+ = 2723 Jy and a spectral index &alpha. = -0.770 (epoch 1980.0) (Baars et al., 1977). See Kuehr et al. (1981) for a discussion of the details of the selection and compilation of flux densities. See also refs.dat Jy e_flux-1 Flux density error The flux density measurements are listed, in rows, in order of ascending frequency, so that consecutive frequencies run from left to right. The data may be read in ascending frequency order by using a repeating FORTRAN format statement to read successive records. All flux densities given . . . are on the scale of Baars et al. (1977). This scale is based on the absolute radio spectrum of Cassiopeia A. Between 0.3 and 30 GHz it is given by a flux density S+ = 2723 Jy and a spectral index &alpha. = -0.770 (epoch 1980.0) (Baars et al., 1977). See Kuehr et al. (1981) for a discussion of the details of the selection and compilation of flux densities. See also refs.dat Flux density errors were either taken directly from the catalogue or were calculated according to the formulae given there. Jy ref-1 Reference number This is the code number for the radio source catalog from which the particular flux density measurement came. refs.dat contains the radio source catalogs used and their attributes, sorted by code number. In one case the original catalog listed no source catalog and this field is blank. One source catalog code number (number 94) has three distinct catalogs associated with it, which are differentiated by , A, or B in this field. In all other cases this field is blank. --- ref-1-s Ref. number suffix This is the code number for the radio source catalog from which the particular flux density measurement came. refs.dat contains the radio source catalogs used and their attributes, sorted by code number. In one case the original catalog listed no source catalog and this field is blank. One source catalog code number (number 94) has three distinct catalogs associated with it, which are differentiated by , A, or B in this field. In all other cases this field is blank. --- freq-2 Frequency Hz col-2 --- flux-2 Flux density The flux density measurements are listed, in rows, in order of ascending frequency, so that consecutive frequencies run from left to right. The data may be read in ascending frequency order by using a repeating FORTRAN format statement to read successive records. All flux densities given . . . are on the scale of Baars et al. (1977). This scale is based on the absolute radio spectrum of Cassiopeia A. Between 0.3 and 30 GHz it is given by a flux density S+ = 2723 Jy and a spectral index &alpha. = -0.770 (epoch 1980.0) (Baars et al., 1977). See Kuehr et al. (1981) for a discussion of the details of the selection and compilation of flux densities. See also refs.dat Jy e_flux-2 Flux density error The flux density measurements are listed, in rows, in order of ascending frequency, so that consecutive frequencies run from left to right. The data may be read in ascending frequency order by using a repeating FORTRAN format statement to read successive records. All flux densities given . . . are on the scale of Baars et al. (1977). This scale is based on the absolute radio spectrum of Cassiopeia A. Between 0.3 and 30 GHz it is given by a flux density S+ = 2723 Jy and a spectral index &alpha. = -0.770 (epoch 1980.0) (Baars et al., 1977). See Kuehr et al. (1981) for a discussion of the details of the selection and compilation of flux densities. See also refs.dat Flux density errors were either taken directly from the catalogue or were calculated according to the formulae given there. Jy ref-2 Reference number This is the code number for the radio source catalog from which the particular flux density measurement came. refs.dat contains the radio source catalogs used and their attributes, sorted by code number. In one case the original catalog listed no source catalog and this field is blank. One source catalog code number (number 94) has three distinct catalogs associated with it, which are differentiated by , A, or B in this field. In all other cases this field is blank. --- ref-2-s Ref. number suffix This is the code number for the radio source catalog from which the particular flux density measurement came. refs.dat contains the radio source catalogs used and their attributes, sorted by code number. In one case the original catalog listed no source catalog and this field is blank. One source catalog code number (number 94) has three distinct catalogs associated with it, which are differentiated by , A, or B in this field. In all other cases this field is blank. --- freq-3 Frequency Hz col-3 --- flux-3 Flux density The flux density measurements are listed, in rows, in order of ascending frequency, so that consecutive frequencies run from left to right. The data may be read in ascending frequency order by using a repeating FORTRAN format statement to read successive records. All flux densities given . . . are on the scale of Baars et al. (1977). This scale is based on the absolute radio spectrum of Cassiopeia A. Between 0.3 and 30 GHz it is given by a flux density S+ = 2723 Jy and a spectral index &alpha. = -0.770 (epoch 1980.0) (Baars et al., 1977). See Kuehr et al. (1981) for a discussion of the details of the selection and compilation of flux densities. See also refs.dat Jy e_flux-3 Flux density error The flux density measurements are listed, in rows, in order of ascending frequency, so that consecutive frequencies run from left to right. The data may be read in ascending frequency order by using a repeating FORTRAN format statement to read successive records. All flux densities given . . . are on the scale of Baars et al. (1977). This scale is based on the absolute radio spectrum of Cassiopeia A. Between 0.3 and 30 GHz it is given by a flux density S+ = 2723 Jy and a spectral index &alpha. = -0.770 (epoch 1980.0) (Baars et al., 1977). See Kuehr et al. (1981) for a discussion of the details of the selection and compilation of flux densities. See also refs.dat Flux density errors were either taken directly from the catalogue or were calculated according to the formulae given there. Jy ref-3 Reference number This is the code number for the radio source catalog from which the particular flux density measurement came. refs.dat contains the radio source catalogs used and their attributes, sorted by code number. In one case the original catalog listed no source catalog and this field is blank. One source catalog code number (number 94) has three distinct catalogs associated with it, which are differentiated by , A, or B in this field. In all other cases this field is blank. --- ref-3-s Ref. number suffix This is the code number for the radio source catalog from which the particular flux density measurement came. refs.dat contains the radio source catalogs used and their attributes, sorted by code number. In one case the original catalog listed no source catalog and this field is blank. One source catalog code number (number 94) has three distinct catalogs associated with it, which are differentiated by , A, or B in this field. In all other cases this field is blank. --- freq-4 Frequency Hz col-4 --- flux-4 Flux density The flux density measurements are listed, in rows, in order of ascending frequency, so that consecutive frequencies run from left to right. The data may be read in ascending frequency order by using a repeating FORTRAN format statement to read successive records. All flux densities given . . . are on the scale of Baars et al. (1977). This scale is based on the absolute radio spectrum of Cassiopeia A. Between 0.3 and 30 GHz it is given by a flux density S+ = 2723 Jy and a spectral index &alpha. = -0.770 (epoch 1980.0) (Baars et al., 1977). See Kuehr et al. (1981) for a discussion of the details of the selection and compilation of flux densities. See also refs.dat Jy e_flux-4 Flux density error The flux density measurements are listed, in rows, in order of ascending frequency, so that consecutive frequencies run from left to right. The data may be read in ascending frequency order by using a repeating FORTRAN format statement to read successive records. All flux densities given . . . are on the scale of Baars et al. (1977). This scale is based on the absolute radio spectrum of Cassiopeia A. Between 0.3 and 30 GHz it is given by a flux density S+ = 2723 Jy and a spectral index &alpha. = -0.770 (epoch 1980.0) (Baars et al., 1977). See Kuehr et al. (1981) for a discussion of the details of the selection and compilation of flux densities. See also refs.dat Flux density errors were either taken directly from the catalogue or were calculated according to the formulae given there. Jy ref-4 Reference number This is the code number for the radio source catalog from which the particular flux density measurement came. refs.dat contains the radio source catalogs used and their attributes, sorted by code number. In one case the original catalog listed no source catalog and this field is blank. One source catalog code number (number 94) has three distinct catalogs associated with it, which are differentiated by , A, or B in this field. In all other cases this field is blank. --- ref-4-s Ref. number suffix This is the code number for the radio source catalog from which the particular flux density measurement came. refs.dat contains the radio source catalogs used and their attributes, sorted by code number. In one case the original catalog listed no source catalog and this field is blank. One source catalog code number (number 94) has three distinct catalogs associated with it, which are differentiated by , A, or B in this field. In all other cases this field is blank. --- References code Code number The code numbers appearing in the flux density data records. The file is sorted on this datum. In four cases this field is blank, but the suffix contains an asterisk. This indicates a source catalog not directly referenced in any flux density measurement, but which the authors included in the Radio Source Catalogues list of the original paper. They are included here for completeness and are the first four source catalogs listed in this file. Code numbers 901-910 correspond to unpublished flux densities. If both this and the suffix fields are blank, the reference(s) field will be a continuation from the previous record. --- suf Suffix One code number (number 94) has three distinct source catalogs associated with it, which are differentiated by , A, or B in this field. An asterisk in this field indicates that the source catalog cited was not directly referenced in any flux density measurement, but was listed in the original paper as a source catalog. In all other cases this field is blank. --- freq Frequency Hz fact Conversion fact This field gives the factor used to convert the flux densities in the catalog to the scale used (Baars et al. 1977) It is a ratio of the Baars et al. (1977) flux density scale to that of the source catalog at the frequency specified. --- flux Flux density limit Jy name-1 Name 1 If the catalog has a common designation (3C, PKs, etc.), it is listed here. --- name-2 Name 2 If the catalog has a common designation (3C, PKs, etc.), it is listed here. --- ref Reference(s) The original paper or papers in which the catalog appeared. There are a maximum of three references for a single catalog. --- Nancy G. Roman ADC/SSDOO 1995 Jul 22 UNKNOWN UNKNOWN The Catalog of Extragalactic Radio Sources Having Flux Densities Greater Than 1 Jy at 5 GHz (EGRS) was sent to the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, by the Centre de Donnees Stellaires (CDS), and received February 10, 1986. The original tape contained a single text file formatted in the same manner as the published catalog; that is, with two header records per object and with the flux density measurements arranged in ascending order in columnar format. The two header records per object were combined into a single record. A FORTRAN program was written to rearrange the flux density measurements from columns into rows, so that the data may now be read in order of ascending flux by using a simple repeating FORTRAN format statement. A FORTRAN program was run that checked the validity of each field according to its data type and value. ADC personnel created a separate file for the radio source catalogs. The data for this file were taken from Kuehr et al. (1981). This work was supervised by Wayne W. Warren who also wrote the original document. To permit every line in the catalog to be read with the same format, the undersigned removed the header lines into a separate file (header.dat) and entered the source id in the first field of each record in catalog.dat. She also translated the document from Script to ASCII and rearranged it into the current standard form and altered the format tables appropriately. UNKNOWN UNKNOWN For each position given in the header records of the catalog file there is also given a two letter code indicating the reference for this position. Codes from AA through BL . . . denote positions measured with a radio interometer, whereas codes SA through SP denote positions from the original survey instrument. The following table defines the codes and the corresponding references. the original survey instrument. AA = VLA calibrator list, Johnston, K., private communication. AB = Adgie, R. L. 1974, Astron. J., 79, 846. AC = Adgie, R. L., Crowther, J. H., Gent, H. 1972, Mon. Not. Roy. Astron. Soc., 159, 233. AD = Adgie, R. L., Gent, H. 1966, Nature, 209, 549. AE = Brandie, G. W., Bridle, A. H. 1974, Astron. J., 79, 903. AF = Bridle, A. H., Fomalont, E. B. 1978, Astron. J., 83, 704. AG = Brosche, P., Wade, C. M., Hjellming, R. M. 1973, Astrophys. J., 183, 805. AH = Cohen, M. H. 1972, Astrophys. Letters, 122, 81 AI = Cohen, A. M., Porcas, R. W., Browne, I. W. A., Daintree, E. J., Walsh, D. 1977, Mem. Roy. Astron. Soc., 84, 1. AJ = Condon, J. J., Hicks, P. D., Jauncey, D. L. 1977, Astron. J., 82, 692. AK = Condon, J. J., Jauncey, D. L., Wright, A. E., 1978, Astron. J., 83, 1036. AL = Douglas, J. N., Bash, F. N., Ghigo, F. D., Moseley, G. F., Torrence, G. W. 1973, Astron. J., 78, 1. AM = Edwards, T., Kronberg, P. P., Menard, G. 1975, Astron. J., 80, 1005. AN = Elsmore, B., Ryle, M. 1976, Mon. Not. Roy. Astron. Soc., 174, 411 AO = Fomalont, E. B., Moffet, A. T. 1971, Astron. J., 76, 5. AP = Right Ascension taken from Fomalont, E. B., Moffet, A. T. 1971, Astron. J., 76, 5. Declination taken from Bolton, J. G., Shimmins, A. J. 1973, Austr. J. Phys. Astrophys. Suppl., 30, 1. AQ = Frater, R. H., Watkinson, A., Retallack, D. S., Goss, W. M. 1976, Mon. Not. Roy. Astron. Soc., 176, 487. AR = Ghigo, F. D. 1977, Astrophys. J. Suppl., 35, 359 AS = Ghigo, F. D., Owen, F. N. 1973, Astron. J., 78, 848. AT = Grueff, G., Vigotti, M. 1975, Astron. Astrophys. Suppl. Ser., 19, 117. AU = Gubbay, J. S. 1978, Astron. J., 83, 697. AV = Haynes, M., Sramek, R. 1975, Astron. J., 80, 673. AW = Hoegbom, J. A., Carlsson, I. 1974, Astron. Astrophys., 34, 341. AX = Hoskins, D. G., Murdoch, H. S., Adgie, R. L., Crowther, J. H., Gent, H. 1974, Mon. Not. Roy. Astron. Soc., 166, 235. AY = Hunstead, R. W., Lasker, B. M., Mintz, B., Smith, M. G. 1971, Austr. J. Phys., 24, 601. AZ = Hunstead, R. W. 1972, Mon. Not. Roy. Astron. Soc., 157, 367. BA = Hunstead, R. W., Lasker, B. M., Mintz, B., Smith, M. G. 1971, Austr. J. Phys., 24, 601. BB = Lasker, B. M., Smith, M. G. 1974, Austr. J. Phys., 27, 13 BC = MacDonald, G. H., Kenderdine, S., Neville, Ann C. 1968, Mon. Not. Roy. Astron. Soc., 138, 259. BD = McEwan, N. J., Browne, I. W. A., Crowther, J. H. 1975, Mem. Roy. Astron. Soc., 80, 1. BE = Owen, F. N., Porcas, R. W., Neff, Susan G. 1978, Astron. J., 83, 1009. BF = Pooley, G. G., Henbest, S. N. 1974, Mon. Not. Roy. Astron. Soc., 176, 487. BG = Sharp, J. R., Bash, F. N. 1975, Astron. J., 80, 335. BH = Veron, M. P., Veron, P., Adgie, R. L., Gent, H. 1976, Astron. Astrophys., 47, 401. BI = Wade, C. M., Miley, G. K. 1971, Astron. J., 76, 101. BJ = Mackay, C. D. 1969, Mon. Not. Roy. Astron. Soc., 145, 31. BK = Pauliny-Toth, I. I. K., Kellerman, K. I., Davis, M. M., Fomalont, E. B., Shaffer, D. B. 1972, Astron. J., 77, 265. BL = NRAO interferometer positions, unpublished. SA = Pauliny-Toth, I. I. K., Kellerman, K. I., Davis, M. M., Fomalont, E. B., Shaffer, D. B. 1972, Astron. J., 77, 265. SB = Pauliny-Toth, I. I. K., Kellerman, K. I. 1972b, Astron. J., 77, 797. SC = Pauliny-Toth, I. I. K., Witzel, A., Preub, E., Kuehr, H., Kellerman, K. I., Fomalont, E. B., Davis, M. M. 1978, Astron. J., 83, 451. SD = Kuehr, H., Pauliny-Toth, I. I. K., Witzel, A., Schmidt J. 1980, Astron. J., (submitted). SE = Wall, J. V., Cannon, R. D. 1973, Austr. J. Phys. Astrophys. Suppl., 31, 1. SE = Wall, J. V., Cannon, R. D. 1973, Austr. J. Phys. Astrophys. Suppl., SE = Wall, J. V., Cannon, R. D. 1973, Austr. J. Phys. Astrophys. Suppl., 31, 1. SF = Shimmins, A. J., Bolton, J. G. 1972b, Austr. J. Phys. Astrophys. Suppl., 26, 1. SG = Bolton, J. G., Shimmins, A. J. 1973, Austr. J. Phys. Astrophys. Suppl., 30, 1. SH = Shimmins, A. J., Bolton, J. G. 1974, Austr. J. Phys. Astrophys. Suppl., 32, 1. SI = Bolton, J. G., Shimmins, A. J., Wall, J. V. 1975, Austr. J. Phys. Astrophys. Suppl., 34, 1. SJ = Bolton, J. G., Butler, P. W. 1975, Austr. J. Phys. Astrophys. Suppl., 34, 33. SK = Wall, J. V., Shimmins, A. J., Bolton, J. G. 1975, Austr. J. Phys. Astrophys. Suppl., 34, 55. SL = Wall, J. V., Wright, A. E., Bolton, J. G. 1976, Austr. J. Phys. Astrophys. Suppl., 39, 1. SM = Wright, A. E., Savage, A., Bolton, J. G. 1977, Austr. J. Phys. Astrophys. Suppl., 41, 1. SN = Savage, A., Wright, A. E., Bolton, J. G. 1977, Austr. J. Phys. Astrophys. Suppl., 44, 1. SO = Bolton, J. G., Wright, A. E., Savage, A. 1979, Austr. J. Phys. Astrophys. Suppl., 46, 1. SP = Shimmins, A. J., Clarke, Margaret E., Ekers, R. D. 1966, Austr. J. Phys., 19, 649. VIII_5.xml The Hat Creek High-Latitude H I Survey 8007A VIII/7A Hat Creek High-Latitude H I Survey The Hat Creek High-Latitude H I Survey C Heiles H J Habing Astron. & Astrophys. Suppl. 14 1 1974 1974A&AS...14....1H Radio sources Surveys H I data This survey consists of H I 21-cm spectra covering the entire northern sky with absolute Galactic latitude |b| >10 degrees and declination dec >-30 degrees. The observations were made with the Hat Creek 85-foot telescope between 1968 and 1970. The individual spectra were obtained with a bank of 100 filters covering the velocity range from -92 km/s to +75 km/s. The velocity resolution was 2 km/sec (except at the ends of the spectra) and the beamwidth was 36 arcmin. The spacing between points observed on the sky is (0.3 deg/cos b) in Galactic longitude and (0.6 deg) in Galactic latitude. A FITS version of the survey was derived at the Astrophysics Data Facility (NASA/GSFC) from the original catalog of spectra. The approximately 130,000 good spectra in the catalog (i.e., those with status code 1 and which have flat baselines) were interpolated to a uniform channel width in frequency, shifted as appropriate to take into account the proper central velocities, then interpolated onto a regular grid in Galactic coordinates. For the latter interpolation, the cos(b) corrections for longitude offsets were taken into account; no interpolation was done across gaps in coverage greater than 2 deg. Latitude-velocity slices were written in FITS format for each 30 arcmin of longitude. Separate files were written for the negative latitude (b < -10 deg ) and positive latitude (b > 10 deg) ranges. Slices containing no spectra, primarily negative latitude spectra in the fourth Galactic quadrant, were not written. A longitude-latitude map, integrated over all velocities, was also written in FITS format to illustrate the coverage of the individual latitude-velocity slices.
Northern sky survey data GLONm Galactic longitude in units of milli- degrees 0.001deg GLATm Galactic latitude in units of milli- degrees 0.001deg RAh Right ascension (B1950) h RAm RA in minutes min RAs RA in seconds s DE- Sign of Declination --- DEd Declination in degrees (B1950) deg DEm DEC in arcminutes arcmin DEs DEC in arcseconds arcsec Datey Date in year date = real(datey) + real(datem-1)/12. + real(dated-1)/(30.6*12.) yr Datem Date in month --- Dated Date in day d LST Local Standard Time s CenVel Central velocity (Local Standard of Rest) m/s Status Status Code The status code included in each spectrum reports the quality of the baseline and the position transcribed to the original tape. If the status word is 1 or 7, the profile should be perfectly good. If the status code is 5 or 8, the profile may be good for some purposes. Status Number of code Spectrum meaning 1 133095 good spectrum 4 322 bad spectrum 5 887 galactic longitude may not be as intended 6 277 position may not be as intended 7 103 calibration missing for this profile 8 176 baseline is not good 9 72 both 5 and 6 apply --- AntTemp 100 antenna temperature of 6 bytes each 0.01K lbmap.fit Velocity-integrated map of the whole plane vb_720p.fit Lat.-vel. map for l = -180.0 deg, b > +10 deg vb_720n.fit Lat.-vel. map for l = -180.0 deg, b < -10 deg vb_001n.fit Lat.-vel. map for l = -179.5 deg, b < -10 deg vb_001p.fit Lat.-vel. map for l = -179.5 deg, b > +10 deg vb_002p.fit Lat.-vel. map for l = -179.0 deg, b > +10 deg vb_002n.fit Lat.-vel. map for l = -179.0 deg, b < -10 deg vb_003n.fit Lat.-vel. map for l = -178.5 deg, b < -10 deg vb_003p.fit Lat.-vel. map for l = -178.5 deg, b > +10 deg vb_004n.fit Lat.-vel. map for l = -178.0 deg, b < -10 deg vb_004p.fit Lat.-vel. map for l = -178.0 deg, b > +10 deg vb_005n.fit Lat.-vel. map for l = -177.5 deg, b < -10 deg vb_005p.fit Lat.-vel. map for l = -177.5 deg, b > +10 deg vb_006n.fit Lat.-vel. map for l = -177.0 deg, b < -10 deg vb_006p.fit Lat.-vel. map for l = -177.0 deg, b > +10 deg vb_007p.fit Lat.-vel. map for l = -176.5 deg, b > +10 deg vb_007n.fit Lat.-vel. map for l = -176.5 deg, b < -10 deg vb_008p.fit Lat.-vel. map for l = -176.0 deg, b > +10 deg vb_008n.fit Lat.-vel. map for l = -176.0 deg, b < -10 deg vb_009p.fit Lat.-vel. map for l = -175.5 deg, b > +10 deg vb_009n.fit Lat.-vel. map for l = -175.5 deg, b < -10 deg vb_010n.fit Lat.-vel. map for l = -175.0 deg, b < -10 deg vb_010p.fit Lat.-vel. map for l = -175.0 deg, b > +10 deg vb_011p.fit Lat.-vel. map for l = -174.5 deg, b > +10 deg vb_011n.fit Lat.-vel. map for l = -174.5 deg, b < -10 deg vb_012p.fit Lat.-vel. map for l = -174.0 deg, b > +10 deg vb_012n.fit Lat.-vel. map for l = -174.0 deg, b < -10 deg vb_013n.fit Lat.-vel. map for l = -173.5 deg, b < -10 deg vb_013p.fit Lat.-vel. map for l = -173.5 deg, b > +10 deg vb_014n.fit Lat.-vel. map for l = -173.0 deg, b < -10 deg vb_014p.fit Lat.-vel. map for l = -173.0 deg, b > +10 deg vb_015n.fit Lat.-vel. map for l = -172.5 deg, b < -10 deg vb_015p.fit Lat.-vel. map for l = -172.5 deg, b > +10 deg vb_016n.fit Lat.-vel. map for l = -172.0 deg, b < -10 deg vb_016p.fit Lat.-vel. map for l = -172.0 deg, b > +10 deg vb_017p.fit Lat.-vel. map for l = -171.5 deg, b > +10 deg vb_017n.fit Lat.-vel. map for l = -171.5 deg, b < -10 deg vb_018p.fit Lat.-vel. map for l = -171.0 deg, b > +10 deg vb_018n.fit Lat.-vel. map for l = -171.0 deg, b < -10 deg vb_019p.fit Lat.-vel. map for l = -170.5 deg, b > +10 deg vb_019n.fit Lat.-vel. map for l = -170.5 deg, b < -10 deg vb_020p.fit Lat.-vel. map for l = -170.0 deg, b > +10 deg vb_020n.fit Lat.-vel. map for l = -170.0 deg, b < -10 deg vb_021n.fit Lat.-vel. map for l = -169.5 deg, b < -10 deg vb_021p.fit Lat.-vel. map for l = -169.5 deg, b > +10 deg vb_022p.fit Lat.-vel. map for l = -169.0 deg, b > +10 deg vb_022n.fit Lat.-vel. map for l = -169.0 deg, b < -10 deg vb_023p.fit Lat.-vel. map for l = -168.5 deg, b > +10 deg vb_023n.fit Lat.-vel. map for l = -168.5 deg, b < -10 deg vb_024p.fit Lat.-vel. map for l = -168.0 deg, b > +10 deg vb_024n.fit Lat.-vel. map for l = -168.0 deg, b < -10 deg vb_025n.fit Lat.-vel. map for l = -167.5 deg, b < -10 deg vb_025p.fit Lat.-vel. map for l = -167.5 deg, b > +10 deg vb_026p.fit Lat.-vel. map for l = -167.0 deg, b > +10 deg vb_026n.fit Lat.-vel. map for l = -167.0 deg, b < -10 deg vb_027p.fit Lat.-vel. map for l = -166.5 deg, b > +10 deg vb_027n.fit Lat.-vel. map for l = -166.5 deg, b < -10 deg vb_028p.fit Lat.-vel. map for l = -166.0 deg, b > +10 deg vb_028n.fit Lat.-vel. map for l = -166.0 deg, b < -10 deg vb_029p.fit Lat.-vel. map for l = -165.5 deg, b > +10 deg vb_029n.fit Lat.-vel. map for l = -165.5 deg, b < -10 deg vb_030p.fit Lat.-vel. map for l = -165.0 deg, b > +10 deg vb_030n.fit Lat.-vel. map for l = -165.0 deg, b < -10 deg vb_031p.fit Lat.-vel. map for l = -164.5 deg, b > +10 deg vb_031n.fit Lat.-vel. map for l = -164.5 deg, b < -10 deg vb_032p.fit Lat.-vel. map for l = -164.0 deg, b > +10 deg vb_032n.fit Lat.-vel. map for l = -164.0 deg, b < -10 deg vb_033p.fit Lat.-vel. map for l = -163.5 deg, b > +10 deg vb_033n.fit Lat.-vel. map for l = -163.5 deg, b < -10 deg vb_034p.fit Lat.-vel. map for l = -163.0 deg, b > +10 deg vb_034n.fit Lat.-vel. map for l = -163.0 deg, b < -10 deg vb_035p.fit Lat.-vel. map for l = -162.5 deg, b > +10 deg vb_035n.fit Lat.-vel. map for l = -162.5 deg, b < -10 deg vb_036p.fit Lat.-vel. map for l = -162.0 deg, b > +10 deg vb_036n.fit Lat.-vel. map for l = -162.0 deg, b < -10 deg vb_037p.fit Lat.-vel. map for l = -161.5 deg, b > +10 deg vb_037n.fit Lat.-vel. map for l = -161.5 deg, b < -10 deg vb_038p.fit Lat.-vel. map for l = -161.0 deg, b > +10 deg vb_038n.fit Lat.-vel. map for l = -161.0 deg, b < -10 deg vb_039p.fit Lat.-vel. map for l = -160.5 deg, b > +10 deg vb_039n.fit Lat.-vel. map for l = -160.5 deg, b < -10 deg vb_040p.fit Lat.-vel. map for l = -160.0 deg, b > +10 deg vb_040n.fit Lat.-vel. map for l = -160.0 deg, b < -10 deg vb_041p.fit Lat.-vel. map for l = -159.5 deg, b > +10 deg vb_041n.fit Lat.-vel. map for l = -159.5 deg, b < -10 deg vb_042p.fit Lat.-vel. map for l = -159.0 deg, b > +10 deg vb_042n.fit Lat.-vel. map for l = -159.0 deg, b < -10 deg vb_043p.fit Lat.-vel. map for l = -158.5 deg, b > +10 deg vb_043n.fit Lat.-vel. map for l = -158.5 deg, b < -10 deg vb_044p.fit Lat.-vel. map for l = -158.0 deg, b > +10 deg vb_044n.fit Lat.-vel. map for l = -158.0 deg, b < -10 deg vb_045p.fit Lat.-vel. map for l = -157.5 deg, b > +10 deg vb_045n.fit Lat.-vel. map for l = -157.5 deg, b < -10 deg vb_046p.fit Lat.-vel. map for l = -157.0 deg, b > +10 deg vb_046n.fit Lat.-vel. map for l = -157.0 deg, b < -10 deg vb_047p.fit Lat.-vel. map for l = -156.5 deg, b > +10 deg vb_047n.fit Lat.-vel. map for l = -156.5 deg, b < -10 deg vb_048p.fit Lat.-vel. map for l = -156.0 deg, b > +10 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vb_057p.fit Lat.-vel. map for l = -151.5 deg, b > +10 deg vb_057n.fit Lat.-vel. map for l = -151.5 deg, b < -10 deg vb_058p.fit Lat.-vel. map for l = -151.0 deg, b > +10 deg vb_058n.fit Lat.-vel. map for l = -151.0 deg, b < -10 deg vb_059p.fit Lat.-vel. map for l = -150.5 deg, b > +10 deg vb_059n.fit Lat.-vel. map for l = -150.5 deg, b < -10 deg vb_060p.fit Lat.-vel. map for l = -150.0 deg, b > +10 deg vb_060n.fit Lat.-vel. map for l = -150.0 deg, b < -10 deg vb_061p.fit Lat.-vel. map for l = -149.5 deg, b > +10 deg vb_061n.fit Lat.-vel. map for l = -149.5 deg, b < -10 deg vb_062p.fit Lat.-vel. map for l = -149.0 deg, b > +10 deg vb_062n.fit Lat.-vel. map for l = -149.0 deg, b < -10 deg vb_063p.fit Lat.-vel. map for l = -148.5 deg, b > +10 deg vb_063n.fit Lat.-vel. map for l = -148.5 deg, b < -10 deg vb_064p.fit Lat.-vel. map for l = -148.0 deg, b > +10 deg vb_064n.fit Lat.-vel. map for l = -148.0 deg, b < -10 deg vb_065n.fit Lat.-vel. map for l = -147.5 deg, b < -10 deg vb_065p.fit Lat.-vel. map for l = -147.5 deg, b > +10 deg vb_066p.fit Lat.-vel. map for l = -147.0 deg, b > +10 deg vb_066n.fit Lat.-vel. map for l = -147.0 deg, b < -10 deg vb_067p.fit Lat.-vel. map for l = -146.5 deg, b > +10 deg vb_067n.fit Lat.-vel. map for l = -146.5 deg, b < -10 deg vb_068p.fit Lat.-vel. map for l = -146.0 deg, b > +10 deg vb_068n.fit Lat.-vel. map for l = -146.0 deg, b < -10 deg vb_069p.fit Lat.-vel. map for l = -145.5 deg, b > +10 deg vb_069n.fit Lat.-vel. map for l = -145.5 deg, b < -10 deg vb_070p.fit Lat.-vel. map for l = -145.0 deg, b > +10 deg vb_070n.fit Lat.-vel. map for l = -145.0 deg, b < -10 deg vb_071p.fit Lat.-vel. map for l = -144.5 deg, b > +10 deg vb_071n.fit Lat.-vel. map for l = -144.5 deg, b < -10 deg vb_072p.fit Lat.-vel. map for l = -144.0 deg, b > +10 deg vb_072n.fit Lat.-vel. map for l = -144.0 deg, b < -10 deg vb_073p.fit Lat.-vel. map for l = -143.5 deg, b > +10 deg vb_073n.fit Lat.-vel. map for l = -143.5 deg, b < -10 deg vb_074p.fit Lat.-vel. map for l = -143.0 deg, b > +10 deg vb_074n.fit Lat.-vel. map for l = -143.0 deg, b < -10 deg vb_075p.fit Lat.-vel. map for l = -142.5 deg, b > +10 deg vb_075n.fit Lat.-vel. map for l = -142.5 deg, b < -10 deg vb_076p.fit Lat.-vel. map for l = -142.0 deg, b > +10 deg vb_076n.fit Lat.-vel. map for l = -142.0 deg, b < -10 deg vb_077p.fit Lat.-vel. map for l = -141.5 deg, b > +10 deg vb_077n.fit Lat.-vel. map for l = -141.5 deg, b < -10 deg vb_078p.fit Lat.-vel. map for l = -141.0 deg, b > +10 deg vb_078n.fit Lat.-vel. map for l = -141.0 deg, b < -10 deg vb_079p.fit Lat.-vel. map for l = -140.5 deg, b > +10 deg vb_079n.fit Lat.-vel. map for l = -140.5 deg, b < -10 deg vb_080p.fit Lat.-vel. map for l = -140.0 deg, b > +10 deg vb_080n.fit Lat.-vel. map for l = -140.0 deg, b < -10 deg vb_081p.fit Lat.-vel. map for l = -139.5 deg, b > +10 deg vb_081n.fit Lat.-vel. map for l = -139.5 deg, b < -10 deg vb_082p.fit Lat.-vel. map for l = -139.0 deg, b > +10 deg vb_082n.fit Lat.-vel. map for l = -139.0 deg, b < -10 deg vb_083p.fit Lat.-vel. map for l = -138.5 deg, b > +10 deg vb_083n.fit Lat.-vel. map for l = -138.5 deg, b < -10 deg vb_084p.fit Lat.-vel. map for l = -138.0 deg, b > +10 deg vb_084n.fit Lat.-vel. map for l = -138.0 deg, b < -10 deg vb_085p.fit Lat.-vel. map for l = -137.5 deg, b > +10 deg vb_085n.fit Lat.-vel. map for l = -137.5 deg, b < -10 deg vb_086p.fit Lat.-vel. map for l = -137.0 deg, b > +10 deg vb_086n.fit Lat.-vel. map for l = -137.0 deg, b < -10 deg vb_087p.fit Lat.-vel. map for l = -136.5 deg, b > +10 deg vb_087n.fit Lat.-vel. map for l = -136.5 deg, b < -10 deg vb_088p.fit Lat.-vel. map for l = -136.0 deg, b > +10 deg vb_088n.fit Lat.-vel. map for l = -136.0 deg, b < -10 deg vb_089p.fit Lat.-vel. map for l = -135.5 deg, b > +10 deg vb_089n.fit Lat.-vel. map for l = -135.5 deg, b < -10 deg vb_090p.fit Lat.-vel. map for l = -135.0 deg, b > +10 deg vb_090n.fit Lat.-vel. map for l = -135.0 deg, b < -10 deg vb_091p.fit Lat.-vel. map for l = -134.5 deg, b > +10 deg vb_091n.fit Lat.-vel. map for l = -134.5 deg, b < -10 deg vb_092p.fit Lat.-vel. map for l = -134.0 deg, b > +10 deg vb_092n.fit Lat.-vel. map for l = -134.0 deg, b < -10 deg vb_093p.fit Lat.-vel. map for l = -133.5 deg, b > +10 deg vb_093n.fit Lat.-vel. map for l = -133.5 deg, b < -10 deg vb_094p.fit Lat.-vel. map for l = -133.0 deg, b > +10 deg vb_094n.fit Lat.-vel. map for l = -133.0 deg, b < -10 deg vb_095p.fit Lat.-vel. map for l = -132.5 deg, b > +10 deg vb_095n.fit Lat.-vel. map for l = -132.5 deg, b < -10 deg vb_096p.fit Lat.-vel. map for l = -132.0 deg, b > +10 deg vb_096n.fit Lat.-vel. map for l = -132.0 deg, b < -10 deg vb_097p.fit Lat.-vel. map for l = -131.5 deg, b > +10 deg vb_097n.fit Lat.-vel. map for l = -131.5 deg, b < -10 deg vb_098p.fit Lat.-vel. map for l = -131.0 deg, b > +10 deg vb_098n.fit Lat.-vel. map for l = -131.0 deg, b < -10 deg vb_099p.fit Lat.-vel. map for l = -130.5 deg, b > +10 deg vb_099n.fit Lat.-vel. map for l = -130.5 deg, b < -10 deg vb_100p.fit Lat.-vel. map for l = -130.0 deg, b > +10 deg vb_100n.fit Lat.-vel. map for l = -130.0 deg, b < -10 deg vb_101p.fit Lat.-vel. map for l = -129.5 deg, b > +10 deg vb_101n.fit Lat.-vel. map for l = -129.5 deg, b < -10 deg vb_102p.fit Lat.-vel. map for l = -129.0 deg, b > +10 deg vb_102n.fit Lat.-vel. map for l = -129.0 deg, b < -10 deg vb_103p.fit Lat.-vel. map for l = -128.5 deg, b > +10 deg vb_103n.fit Lat.-vel. map for l = -128.5 deg, b < -10 deg vb_104p.fit Lat.-vel. map for l = -128.0 deg, b > +10 deg vb_104n.fit Lat.-vel. map for l = -128.0 deg, b < -10 deg vb_105p.fit Lat.-vel. map for l = -127.5 deg, b > +10 deg vb_105n.fit Lat.-vel. map for l = -127.5 deg, b < -10 deg vb_106p.fit Lat.-vel. map for l = -127.0 deg, b > +10 deg vb_106n.fit Lat.-vel. map for l = -127.0 deg, b < -10 deg vb_107p.fit Lat.-vel. map for l = -126.5 deg, b > +10 deg vb_107n.fit Lat.-vel. map for l = -126.5 deg, b < -10 deg vb_108p.fit Lat.-vel. map for l = -126.0 deg, b > +10 deg vb_108n.fit Lat.-vel. map for l = -126.0 deg, b < -10 deg vb_109p.fit Lat.-vel. map for l = -125.5 deg, b > +10 deg vb_109n.fit Lat.-vel. map for l = -125.5 deg, b < -10 deg vb_110p.fit Lat.-vel. map for l = -125.0 deg, b > +10 deg vb_110n.fit Lat.-vel. map for l = -125.0 deg, b < -10 deg vb_111p.fit Lat.-vel. map for l = -124.5 deg, b > +10 deg vb_111n.fit Lat.-vel. map for l = -124.5 deg, b < -10 deg vb_112p.fit Lat.-vel. map for l = -124.0 deg, b > +10 deg vb_112n.fit Lat.-vel. map for l = -124.0 deg, b < -10 deg vb_113p.fit Lat.-vel. map for l = -123.5 deg, b > +10 deg vb_113n.fit Lat.-vel. map for l = -123.5 deg, b < -10 deg vb_114p.fit Lat.-vel. map for l = -123.0 deg, b > +10 deg vb_114n.fit Lat.-vel. map for l = -123.0 deg, b < -10 deg vb_115p.fit Lat.-vel. map for l = -122.5 deg, b > +10 deg vb_116p.fit Lat.-vel. map for l = -122.0 deg, b > +10 deg vb_117p.fit Lat.-vel. map for l = -121.5 deg, b > +10 deg vb_118p.fit Lat.-vel. map for l = -121.0 deg, b > +10 deg vb_119p.fit Lat.-vel. map for l = -120.5 deg, b > +10 deg vb_120p.fit Lat.-vel. map for l = -120.0 deg, b > +10 deg vb_121p.fit Lat.-vel. map for l = -119.5 deg, b > +10 deg vb_122p.fit Lat.-vel. map for l = -119.0 deg, b > +10 deg vb_123p.fit Lat.-vel. map for l = -118.5 deg, b > +10 deg vb_124p.fit Lat.-vel. map for l = -118.0 deg, b > +10 deg vb_125p.fit Lat.-vel. map for l = -117.5 deg, b > +10 deg vb_126p.fit Lat.-vel. map for l = -117.0 deg, b > +10 deg vb_127p.fit Lat.-vel. map for l = -116.5 deg, b > +10 deg vb_128p.fit Lat.-vel. map for l = -116.0 deg, b > +10 deg vb_129p.fit Lat.-vel. map for l = -115.5 deg, b > +10 deg vb_130p.fit Lat.-vel. map for l = -115.0 deg, b > +10 deg vb_131p.fit Lat.-vel. map for l = -114.5 deg, b > +10 deg vb_132p.fit Lat.-vel. map for l = -114.0 deg, b > +10 deg vb_133p.fit Lat.-vel. map for l = -113.5 deg, b > +10 deg vb_134p.fit Lat.-vel. map for l = -113.0 deg, b > +10 deg vb_135p.fit Lat.-vel. map for l = -112.5 deg, b > +10 deg vb_136p.fit Lat.-vel. map for l = -112.0 deg, b > +10 deg vb_137p.fit Lat.-vel. map for l = -111.5 deg, b > +10 deg vb_138p.fit Lat.-vel. map for l = -111.0 deg, b > +10 deg vb_139p.fit Lat.-vel. map for l = -110.5 deg, b > +10 deg vb_140p.fit Lat.-vel. map for l = -110.0 deg, b > +10 deg vb_141p.fit Lat.-vel. map for l = -109.5 deg, b > +10 deg vb_142p.fit Lat.-vel. map for l = -109.0 deg, b > +10 deg vb_143p.fit Lat.-vel. map for l = -108.5 deg, b > +10 deg vb_144p.fit Lat.-vel. map for l = -108.0 deg, b > +10 deg vb_145p.fit Lat.-vel. map for l = -107.5 deg, b > +10 deg vb_146p.fit Lat.-vel. map for l = -107.0 deg, b > +10 deg vb_147p.fit Lat.-vel. map for l = -106.5 deg, b > +10 deg vb_148p.fit Lat.-vel. map for l = -106.0 deg, b > +10 deg vb_149p.fit Lat.-vel. map for l = -105.5 deg, b > +10 deg vb_150p.fit Lat.-vel. map for l = -105.0 deg, b > +10 deg vb_151p.fit Lat.-vel. map for l = -104.5 deg, b > +10 deg vb_152p.fit Lat.-vel. map for l = -104.0 deg, b > +10 deg vb_153p.fit Lat.-vel. map for l = -103.5 deg, b > +10 deg vb_154p.fit Lat.-vel. map for l = -103.0 deg, b > +10 deg vb_155p.fit Lat.-vel. map for l = -102.5 deg, b > +10 deg vb_156p.fit Lat.-vel. map for l = -102.0 deg, b > +10 deg vb_157p.fit Lat.-vel. map for l = -101.5 deg, b > +10 deg vb_158p.fit Lat.-vel. map for l = -101.0 deg, b > +10 deg vb_159p.fit Lat.-vel. map for l = -100.5 deg, b > +10 deg vb_160p.fit Lat.-vel. map for l = -100.0 deg, b > +10 deg vb_161p.fit Lat.-vel. map for l = -99.5 deg, b > +10 deg vb_162p.fit Lat.-vel. map for l = -99.0 deg, b > +10 deg vb_163p.fit Lat.-vel. map for l = -98.5 deg, b > +10 deg vb_164p.fit Lat.-vel. map for l = -98.0 deg, b > +10 deg vb_165p.fit Lat.-vel. map for l = -97.5 deg, b > +10 deg vb_166p.fit Lat.-vel. map for l = -97.0 deg, b > +10 deg vb_167p.fit Lat.-vel. map for l = -96.5 deg, b > +10 deg vb_168p.fit Lat.-vel. map for l = -96.0 deg, b > +10 deg vb_169p.fit Lat.-vel. map for l = -95.5 deg, b > +10 deg vb_170p.fit Lat.-vel. map for l = -95.0 deg, b > +10 deg vb_171p.fit Lat.-vel. map for l = -94.5 deg, b > +10 deg vb_172p.fit Lat.-vel. map for l = -94.0 deg, b > +10 deg vb_173p.fit Lat.-vel. map for l = -93.5 deg, b > +10 deg vb_174p.fit Lat.-vel. map for l = -93.0 deg, b > +10 deg vb_175p.fit Lat.-vel. map for l = -92.5 deg, b > +10 deg vb_176p.fit Lat.-vel. map for l = -92.0 deg, b > +10 deg vb_177p.fit Lat.-vel. map for l = -91.5 deg, b > +10 deg vb_178p.fit Lat.-vel. map for l = -91.0 deg, b > +10 deg vb_179p.fit Lat.-vel. map for l = -90.5 deg, b > +10 deg vb_180p.fit Lat.-vel. map for l = -90.0 deg, b > +10 deg vb_181p.fit Lat.-vel. map for l = -89.5 deg, b > +10 deg vb_182p.fit Lat.-vel. map for l = -89.0 deg, b > +10 deg vb_183p.fit Lat.-vel. map for l = -88.5 deg, b > +10 deg vb_184p.fit Lat.-vel. map for l = -88.0 deg, b > +10 deg vb_185p.fit Lat.-vel. map for l = -87.5 deg, b > +10 deg vb_186p.fit Lat.-vel. map for l = -87.0 deg, b > +10 deg vb_187p.fit Lat.-vel. map for l = -86.5 deg, b > +10 deg vb_188p.fit Lat.-vel. map for l = -86.0 deg, b > +10 deg vb_189p.fit Lat.-vel. map for l = -85.5 deg, b > +10 deg vb_190p.fit Lat.-vel. map for l = -85.0 deg, b > +10 deg vb_191p.fit Lat.-vel. map for l = -84.5 deg, b > +10 deg vb_192p.fit Lat.-vel. map for l = -84.0 deg, b > +10 deg vb_193p.fit Lat.-vel. map for l = -83.5 deg, b > +10 deg vb_194p.fit Lat.-vel. map for l = -83.0 deg, b > +10 deg vb_195p.fit Lat.-vel. map for l = -82.5 deg, b > +10 deg vb_196p.fit Lat.-vel. map for l = -82.0 deg, b > +10 deg vb_197p.fit Lat.-vel. map for l = -81.5 deg, b > +10 deg vb_198p.fit Lat.-vel. map for l = -81.0 deg, b > +10 deg vb_199p.fit Lat.-vel. map for l = -80.5 deg, b > +10 deg vb_200p.fit Lat.-vel. map for l = -80.0 deg, b > +10 deg vb_201p.fit Lat.-vel. map for l = -79.5 deg, b > +10 deg vb_202p.fit Lat.-vel. map for l = -79.0 deg, b > +10 deg vb_203p.fit Lat.-vel. map for l = -78.5 deg, b > +10 deg vb_204p.fit Lat.-vel. map for l = -78.0 deg, b > +10 deg vb_205p.fit Lat.-vel. map for l = -77.5 deg, b > +10 deg vb_206p.fit Lat.-vel. map for l = -77.0 deg, b > +10 deg vb_207p.fit Lat.-vel. map for l = -76.5 deg, b > +10 deg vb_208p.fit Lat.-vel. map for l = -76.0 deg, b > +10 deg vb_209p.fit Lat.-vel. map for l = -75.5 deg, b > +10 deg vb_210p.fit Lat.-vel. map for l = -75.0 deg, b > +10 deg vb_211p.fit Lat.-vel. map for l = -74.5 deg, b > +10 deg vb_212p.fit Lat.-vel. map for l = -74.0 deg, b > +10 deg vb_213p.fit Lat.-vel. map for l = -73.5 deg, b > +10 deg vb_214p.fit Lat.-vel. map for l = -73.0 deg, b > +10 deg vb_215p.fit Lat.-vel. map for l = -72.5 deg, b > +10 deg vb_216p.fit Lat.-vel. map for l = -72.0 deg, b > +10 deg vb_217p.fit Lat.-vel. map for l = -71.5 deg, b > +10 deg vb_218p.fit Lat.-vel. map for l = -71.0 deg, b > +10 deg vb_219p.fit Lat.-vel. map for l = -70.5 deg, b > +10 deg vb_220p.fit Lat.-vel. map for l = -70.0 deg, b > +10 deg vb_221p.fit Lat.-vel. map for l = -69.5 deg, b > +10 deg vb_222p.fit Lat.-vel. map for l = -69.0 deg, b > +10 deg vb_223p.fit Lat.-vel. map for l = -68.5 deg, b > +10 deg vb_224p.fit Lat.-vel. map for l = -68.0 deg, b > +10 deg vb_225p.fit Lat.-vel. map for l = -67.5 deg, b > +10 deg vb_226p.fit Lat.-vel. map for l = -67.0 deg, b > +10 deg vb_227p.fit Lat.-vel. map for l = -66.5 deg, b > +10 deg vb_228p.fit Lat.-vel. map for l = -66.0 deg, b > +10 deg vb_229p.fit Lat.-vel. map for l = -65.5 deg, b > +10 deg vb_230p.fit Lat.-vel. map for l = -65.0 deg, b > +10 deg vb_231p.fit Lat.-vel. map for l = -64.5 deg, b > +10 deg vb_232p.fit Lat.-vel. map for l = -64.0 deg, b > +10 deg vb_233p.fit Lat.-vel. map for l = -63.5 deg, b > +10 deg vb_234p.fit Lat.-vel. map for l = -63.0 deg, b > +10 deg vb_235p.fit Lat.-vel. map for l = -62.5 deg, b > +10 deg vb_236p.fit Lat.-vel. map for l = -62.0 deg, b > +10 deg vb_237p.fit Lat.-vel. map for l = -61.5 deg, b > +10 deg vb_238p.fit Lat.-vel. map for l = -61.0 deg, b > +10 deg vb_239p.fit Lat.-vel. map for l = -60.5 deg, b > +10 deg vb_240p.fit Lat.-vel. map for l = -60.0 deg, b > +10 deg vb_241p.fit Lat.-vel. map for l = -59.5 deg, b > +10 deg vb_242p.fit Lat.-vel. map for l = -59.0 deg, b > +10 deg vb_243p.fit Lat.-vel. map for l = -58.5 deg, b > +10 deg vb_244p.fit Lat.-vel. map for l = -58.0 deg, b > +10 deg vb_245p.fit Lat.-vel. map for l = -57.5 deg, b > +10 deg vb_246p.fit Lat.-vel. map for l = -57.0 deg, b > +10 deg vb_247p.fit Lat.-vel. map for l = -56.5 deg, b > +10 deg vb_248p.fit Lat.-vel. map for l = -56.0 deg, b > +10 deg vb_249p.fit Lat.-vel. map for l = -55.5 deg, b > +10 deg vb_250p.fit Lat.-vel. map for l = -55.0 deg, b > +10 deg vb_251p.fit Lat.-vel. map for l = -54.5 deg, b > +10 deg vb_252p.fit Lat.-vel. map for l = -54.0 deg, b > +10 deg vb_253p.fit Lat.-vel. map for l = -53.5 deg, b > +10 deg vb_254p.fit Lat.-vel. map for l = -53.0 deg, b > +10 deg vb_255p.fit Lat.-vel. map for l = -52.5 deg, b > +10 deg vb_256p.fit Lat.-vel. map for l = -52.0 deg, b > +10 deg vb_257p.fit Lat.-vel. map for l = -51.5 deg, b > +10 deg vb_258p.fit Lat.-vel. map for l = -51.0 deg, b > +10 deg vb_259p.fit Lat.-vel. map for l = -50.5 deg, b > +10 deg vb_260p.fit Lat.-vel. map for l = -50.0 deg, b > +10 deg vb_261p.fit Lat.-vel. map for l = -49.5 deg, b > +10 deg vb_262p.fit Lat.-vel. map for l = -49.0 deg, b > +10 deg vb_263p.fit Lat.-vel. map for l = -48.5 deg, b > +10 deg vb_264p.fit Lat.-vel. map for l = -48.0 deg, b > +10 deg vb_265p.fit Lat.-vel. map for l = -47.5 deg, b > +10 deg vb_266p.fit Lat.-vel. map for l = -47.0 deg, b > +10 deg vb_267p.fit Lat.-vel. map for l = -46.5 deg, b > +10 deg vb_268p.fit Lat.-vel. map for l = -46.0 deg, b > +10 deg vb_269p.fit Lat.-vel. map for l = -45.5 deg, b > +10 deg vb_270p.fit Lat.-vel. map for l = -45.0 deg, b > +10 deg vb_271p.fit Lat.-vel. map for l = -44.5 deg, b > +10 deg vb_272p.fit Lat.-vel. map for l = -44.0 deg, b > +10 deg vb_273p.fit Lat.-vel. map for l = -43.5 deg, b > +10 deg vb_274p.fit Lat.-vel. map for l = -43.0 deg, b > +10 deg vb_275p.fit Lat.-vel. map for l = -42.5 deg, b > +10 deg vb_276p.fit Lat.-vel. map for l = -42.0 deg, b > +10 deg vb_277p.fit Lat.-vel. map for l = -41.5 deg, b > +10 deg vb_278p.fit Lat.-vel. map for l = -41.0 deg, b > +10 deg vb_279p.fit Lat.-vel. map for l = -40.5 deg, b > +10 deg vb_280p.fit Lat.-vel. map for l = -40.0 deg, b > +10 deg vb_281p.fit Lat.-vel. map for l = -39.5 deg, b > +10 deg vb_282p.fit Lat.-vel. map for l = -39.0 deg, b > +10 deg vb_283p.fit Lat.-vel. map for l = -38.5 deg, b > +10 deg vb_284p.fit Lat.-vel. map for l = -38.0 deg, b > +10 deg vb_285p.fit Lat.-vel. map for l = -37.5 deg, b > +10 deg vb_286p.fit Lat.-vel. map for l = -37.0 deg, b > +10 deg vb_287p.fit Lat.-vel. map for l = -36.5 deg, b > +10 deg vb_288p.fit Lat.-vel. map for l = -36.0 deg, b > +10 deg vb_289p.fit Lat.-vel. map for l = -35.5 deg, b > +10 deg vb_290p.fit Lat.-vel. map for l = -35.0 deg, b > +10 deg vb_291p.fit Lat.-vel. map for l = -34.5 deg, b > +10 deg vb_292p.fit Lat.-vel. map for l = -34.0 deg, b > +10 deg vb_293p.fit Lat.-vel. map for l = -33.5 deg, b > +10 deg vb_294p.fit Lat.-vel. map for l = -33.0 deg, b > +10 deg vb_295p.fit Lat.-vel. map for l = -32.5 deg, b > +10 deg vb_296p.fit Lat.-vel. map for l = -32.0 deg, b > +10 deg vb_297p.fit Lat.-vel. map for l = -31.5 deg, b > +10 deg vb_298p.fit Lat.-vel. map for l = -31.0 deg, b > +10 deg vb_299p.fit Lat.-vel. map for l = -30.5 deg, b > +10 deg vb_300p.fit Lat.-vel. map for l = -30.0 deg, b > +10 deg vb_301p.fit Lat.-vel. map for l = -29.5 deg, b > +10 deg vb_302p.fit Lat.-vel. map for l = -29.0 deg, b > +10 deg vb_303p.fit Lat.-vel. map for l = -28.5 deg, b > +10 deg vb_304p.fit Lat.-vel. map for l = -28.0 deg, b > +10 deg vb_305p.fit Lat.-vel. map for l = -27.5 deg, b > +10 deg vb_306p.fit Lat.-vel. map for l = -27.0 deg, b > +10 deg vb_307p.fit Lat.-vel. map for l = -26.5 deg, b > +10 deg vb_308p.fit Lat.-vel. map for l = -26.0 deg, b > +10 deg vb_309p.fit Lat.-vel. map for l = -25.5 deg, b > +10 deg vb_310p.fit Lat.-vel. map for l = -25.0 deg, b > +10 deg vb_311p.fit Lat.-vel. map for l = -24.5 deg, b > +10 deg vb_312p.fit Lat.-vel. map for l = -24.0 deg, b > +10 deg vb_313p.fit Lat.-vel. map for l = -23.5 deg, b > +10 deg vb_314p.fit Lat.-vel. map for l = -23.0 deg, b > +10 deg vb_315p.fit Lat.-vel. map for l = -22.5 deg, b > +10 deg vb_316p.fit Lat.-vel. map for l = -22.0 deg, b > +10 deg vb_317p.fit Lat.-vel. map for l = -21.5 deg, b > +10 deg vb_318p.fit Lat.-vel. map for l = -21.0 deg, b > +10 deg vb_319p.fit Lat.-vel. map for l = -20.5 deg, b > +10 deg vb_320p.fit Lat.-vel. map for l = -20.0 deg, b > +10 deg vb_321p.fit Lat.-vel. map for l = -19.5 deg, b > +10 deg vb_322p.fit Lat.-vel. map for l = -19.0 deg, b > +10 deg vb_323p.fit Lat.-vel. map for l = -18.5 deg, b > +10 deg vb_324p.fit Lat.-vel. map for l = -18.0 deg, b > +10 deg vb_325p.fit Lat.-vel. map for l = -17.5 deg, b > +10 deg vb_326p.fit Lat.-vel. map for l = -17.0 deg, b > +10 deg vb_327p.fit Lat.-vel. map for l = -16.5 deg, b > +10 deg vb_328p.fit Lat.-vel. map for l = -16.0 deg, b > +10 deg vb_329p.fit Lat.-vel. map for l = -15.5 deg, b > +10 deg vb_330p.fit Lat.-vel. map for l = -15.0 deg, b > +10 deg vb_331p.fit Lat.-vel. map for l = -14.5 deg, b > +10 deg vb_332p.fit Lat.-vel. map for l = -14.0 deg, b > +10 deg vb_333p.fit Lat.-vel. map for l = -13.5 deg, b > +10 deg vb_334p.fit Lat.-vel. map for l = -13.0 deg, b > +10 deg vb_335p.fit Lat.-vel. map for l = -12.5 deg, b > +10 deg vb_336p.fit Lat.-vel. map for l = -12.0 deg, b > +10 deg vb_337p.fit Lat.-vel. map for l = -11.5 deg, b > +10 deg vb_338p.fit Lat.-vel. map for l = -11.0 deg, b > +10 deg vb_339p.fit Lat.-vel. map for l = -10.5 deg, b > +10 deg vb_340p.fit Lat.-vel. map for l = -10.0 deg, b > +10 deg vb_341p.fit Lat.-vel. map for l = -9.5 deg, b > +10 deg vb_342p.fit Lat.-vel. map for l = -9.0 deg, b > +10 deg vb_343p.fit Lat.-vel. map for l = -8.5 deg, b > +10 deg vb_344p.fit Lat.-vel. map for l = -8.0 deg, b > +10 deg vb_345p.fit Lat.-vel. map for l = -7.5 deg, b > +10 deg vb_346p.fit Lat.-vel. map for l = -7.0 deg, b > +10 deg vb_347p.fit Lat.-vel. map for l = -6.5 deg, b > +10 deg vb_348p.fit Lat.-vel. map for l = -6.0 deg, b > +10 deg vb_349p.fit Lat.-vel. map for l = -5.5 deg, b > +10 deg vb_350p.fit Lat.-vel. map for l = -5.0 deg, b > +10 deg vb_351p.fit Lat.-vel. map for l = -4.5 deg, b > +10 deg vb_352p.fit Lat.-vel. map for l = -4.0 deg, b > +10 deg vb_353p.fit Lat.-vel. map for l = -3.5 deg, b > +10 deg vb_354p.fit Lat.-vel. map for l = -3.0 deg, b > +10 deg vb_355p.fit Lat.-vel. map for l = -2.5 deg, b > +10 deg vb_356p.fit Lat.-vel. map for l = -2.0 deg, b > +10 deg vb_357p.fit Lat.-vel. map for l = -1.5 deg, b > +10 deg vb_358p.fit Lat.-vel. map for l = -1.0 deg, b > +10 deg vb_359p.fit Lat.-vel. map for l = -0.5 deg, b > +10 deg vb_360p.fit Lat.-vel. map for l = 0.0 deg, b > +10 deg vb_361p.fit Lat.-vel. map for l = 0.5 deg, b > +10 deg vb_362p.fit Lat.-vel. map for l = 1.0 deg, b > +10 deg vb_363p.fit Lat.-vel. map for l = 1.5 deg, b > +10 deg vb_364p.fit Lat.-vel. map for l = 2.0 deg, b > +10 deg vb_365p.fit Lat.-vel. map for l = 2.5 deg, b > +10 deg vb_366p.fit Lat.-vel. map for l = 3.0 deg, b > +10 deg vb_367p.fit Lat.-vel. map for l = 3.5 deg, b > +10 deg vb_368p.fit Lat.-vel. map for l = 4.0 deg, b > +10 deg vb_369p.fit Lat.-vel. map for l = 4.5 deg, b > +10 deg vb_370p.fit Lat.-vel. map for l = 5.0 deg, b > +10 deg vb_371p.fit Lat.-vel. map for l = 5.5 deg, b > +10 deg vb_372p.fit Lat.-vel. map for l = 6.0 deg, b > +10 deg vb_373p.fit Lat.-vel. map for l = 6.5 deg, b > +10 deg vb_374p.fit Lat.-vel. map for l = 7.0 deg, b > +10 deg vb_375p.fit Lat.-vel. map for l = 7.5 deg, b > +10 deg vb_376p.fit Lat.-vel. map for l = 8.0 deg, b > +10 deg vb_377p.fit Lat.-vel. map for l = 8.5 deg, b > +10 deg vb_378n.fit Lat.-vel. map for l = 9.0 deg, b < -10 deg vb_378p.fit Lat.-vel. map for l = 9.0 deg, b > +10 deg vb_379n.fit Lat.-vel. map for l = 9.5 deg, b < -10 deg vb_379p.fit Lat.-vel. map for l = 9.5 deg, b > +10 deg vb_380p.fit Lat.-vel. map for l = 10.0 deg, b > +10 deg vb_380n.fit Lat.-vel. map for l = 10.0 deg, b < -10 deg vb_381p.fit Lat.-vel. map for l = 10.5 deg, b > +10 deg vb_381n.fit Lat.-vel. map for l = 10.5 deg, b < -10 deg vb_382p.fit Lat.-vel. map for l = 11.0 deg, b > +10 deg vb_382n.fit Lat.-vel. map for l = 11.0 deg, b < -10 deg vb_383n.fit Lat.-vel. map for l = 11.5 deg, b < -10 deg vb_383p.fit Lat.-vel. map for l = 11.5 deg, b > +10 deg vb_384p.fit Lat.-vel. map for l = 12.0 deg, b > +10 deg vb_384n.fit Lat.-vel. map for l = 12.0 deg, b < -10 deg vb_385p.fit Lat.-vel. map for l = 12.5 deg, b > +10 deg vb_385n.fit Lat.-vel. map for l = 12.5 deg, b < -10 deg vb_386p.fit Lat.-vel. map for l = 13.0 deg, b > +10 deg vb_386n.fit Lat.-vel. map for l = 13.0 deg, b < -10 deg vb_387n.fit Lat.-vel. map for l = 13.5 deg, b < -10 deg vb_387p.fit Lat.-vel. map for l = 13.5 deg, b > +10 deg vb_388p.fit Lat.-vel. map for l = 14.0 deg, b > +10 deg vb_388n.fit Lat.-vel. map for l = 14.0 deg, b < -10 deg vb_389p.fit Lat.-vel. map for l = 14.5 deg, b > +10 deg vb_389n.fit Lat.-vel. map for l = 14.5 deg, b < -10 deg vb_390p.fit Lat.-vel. map for l = 15.0 deg, b > +10 deg vb_390n.fit Lat.-vel. map for l = 15.0 deg, b < -10 deg vb_391n.fit Lat.-vel. map for l = 15.5 deg, b < -10 deg vb_391p.fit Lat.-vel. map for l = 15.5 deg, b > +10 deg vb_392p.fit Lat.-vel. map for l = 16.0 deg, b > +10 deg vb_392n.fit Lat.-vel. map for l = 16.0 deg, b < -10 deg vb_393p.fit Lat.-vel. map for l = 16.5 deg, b > +10 deg vb_393n.fit Lat.-vel. map for l = 16.5 deg, b < -10 deg vb_394p.fit Lat.-vel. map for l = 17.0 deg, b > +10 deg vb_394n.fit Lat.-vel. map for l = 17.0 deg, b < -10 deg vb_395n.fit Lat.-vel. map for l = 17.5 deg, b < -10 deg vb_395p.fit Lat.-vel. map for l = 17.5 deg, b > +10 deg vb_396p.fit Lat.-vel. map for l = 18.0 deg, b > +10 deg vb_396n.fit Lat.-vel. map for l = 18.0 deg, b < -10 deg vb_397p.fit Lat.-vel. map for l = 18.5 deg, b > +10 deg vb_397n.fit Lat.-vel. map for l = 18.5 deg, b < -10 deg vb_398p.fit Lat.-vel. map for l = 19.0 deg, b > +10 deg vb_398n.fit Lat.-vel. map for l = 19.0 deg, b < -10 deg vb_399n.fit Lat.-vel. map for l = 19.5 deg, b < -10 deg vb_399p.fit Lat.-vel. map for l = 19.5 deg, b > +10 deg vb_400p.fit Lat.-vel. map for l = 20.0 deg, b > +10 deg vb_400n.fit Lat.-vel. map for l = 20.0 deg, b < -10 deg vb_401p.fit Lat.-vel. map for l = 20.5 deg, b > +10 deg vb_401n.fit Lat.-vel. map for l = 20.5 deg, b < -10 deg vb_402p.fit Lat.-vel. map for l = 21.0 deg, b > +10 deg vb_402n.fit Lat.-vel. map for l = 21.0 deg, b < -10 deg vb_403n.fit Lat.-vel. map for l = 21.5 deg, b < -10 deg vb_403p.fit Lat.-vel. map for l = 21.5 deg, b > +10 deg vb_404p.fit Lat.-vel. map for l = 22.0 deg, b > +10 deg vb_404n.fit Lat.-vel. map for l = 22.0 deg, b < -10 deg vb_405p.fit Lat.-vel. map for l = 22.5 deg, b > +10 deg vb_405n.fit Lat.-vel. map for l = 22.5 deg, b < -10 deg vb_406p.fit Lat.-vel. map for l = 23.0 deg, b > +10 deg vb_406n.fit Lat.-vel. map for l = 23.0 deg, b < -10 deg vb_407n.fit Lat.-vel. map for l = 23.5 deg, b < -10 deg vb_407p.fit Lat.-vel. map for l = 23.5 deg, b > +10 deg vb_408p.fit Lat.-vel. map for l = 24.0 deg, b > +10 deg vb_408n.fit Lat.-vel. map for l = 24.0 deg, b < -10 deg vb_409p.fit Lat.-vel. map for l = 24.5 deg, b > +10 deg vb_409n.fit Lat.-vel. map for l = 24.5 deg, b < -10 deg vb_410p.fit Lat.-vel. map for l = 25.0 deg, b > +10 deg vb_410n.fit Lat.-vel. map for l = 25.0 deg, b < -10 deg vb_411n.fit Lat.-vel. map for l = 25.5 deg, b < -10 deg vb_411p.fit Lat.-vel. map for l = 25.5 deg, b > +10 deg vb_412p.fit Lat.-vel. map for l = 26.0 deg, b > +10 deg vb_412n.fit Lat.-vel. map for l = 26.0 deg, b < -10 deg vb_413p.fit Lat.-vel. map for l = 26.5 deg, b > +10 deg vb_413n.fit Lat.-vel. map for l = 26.5 deg, b < -10 deg vb_414p.fit Lat.-vel. map for l = 27.0 deg, b > +10 deg vb_414n.fit Lat.-vel. map for l = 27.0 deg, b < -10 deg vb_415n.fit Lat.-vel. map for l = 27.5 deg, b < -10 deg vb_415p.fit Lat.-vel. map for l = 27.5 deg, b > +10 deg vb_416p.fit Lat.-vel. map for l = 28.0 deg, b > +10 deg vb_416n.fit Lat.-vel. map for l = 28.0 deg, b < -10 deg vb_417p.fit Lat.-vel. map for l = 28.5 deg, b > +10 deg vb_417n.fit Lat.-vel. map for l = 28.5 deg, b < -10 deg vb_418p.fit Lat.-vel. map for l = 29.0 deg, b > +10 deg vb_418n.fit Lat.-vel. map for l = 29.0 deg, b < -10 deg vb_419p.fit Lat.-vel. map for l = 29.5 deg, b > +10 deg vb_419n.fit Lat.-vel. map for l = 29.5 deg, b < -10 deg vb_420p.fit Lat.-vel. map for l = 30.0 deg, b > +10 deg vb_420n.fit Lat.-vel. map for l = 30.0 deg, b < -10 deg vb_421p.fit Lat.-vel. map for l = 30.5 deg, b > +10 deg vb_421n.fit Lat.-vel. map for l = 30.5 deg, b < -10 deg vb_422p.fit Lat.-vel. map for l = 31.0 deg, b > +10 deg vb_422n.fit Lat.-vel. map for l = 31.0 deg, b < -10 deg vb_423n.fit Lat.-vel. map for l = 31.5 deg, b < -10 deg vb_423p.fit Lat.-vel. map for l = 31.5 deg, b > +10 deg vb_424p.fit Lat.-vel. map for l = 32.0 deg, b > +10 deg vb_424n.fit Lat.-vel. map for l = 32.0 deg, b < -10 deg vb_425n.fit Lat.-vel. map for l = 32.5 deg, b < -10 deg vb_425p.fit Lat.-vel. map for l = 32.5 deg, b > +10 deg vb_426p.fit Lat.-vel. map for l = 33.0 deg, b > +10 deg vb_426n.fit Lat.-vel. map for l = 33.0 deg, b < -10 deg vb_427n.fit Lat.-vel. map for l = 33.5 deg, b < -10 deg vb_427p.fit Lat.-vel. map for l = 33.5 deg, b > +10 deg vb_428p.fit Lat.-vel. map for l = 34.0 deg, b > +10 deg vb_428n.fit Lat.-vel. map for l = 34.0 deg, b < -10 deg vb_429p.fit Lat.-vel. map for l = 34.5 deg, b > +10 deg vb_429n.fit Lat.-vel. map for l = 34.5 deg, b < -10 deg vb_430p.fit Lat.-vel. map for l = 35.0 deg, b > +10 deg vb_430n.fit Lat.-vel. map for l = 35.0 deg, b < -10 deg vb_431p.fit Lat.-vel. map for l = 35.5 deg, b > +10 deg vb_431n.fit Lat.-vel. map for l = 35.5 deg, b < -10 deg vb_432p.fit Lat.-vel. map for l = 36.0 deg, b > +10 deg vb_432n.fit Lat.-vel. map for l = 36.0 deg, b < -10 deg vb_433n.fit Lat.-vel. map for l = 36.5 deg, b < -10 deg vb_433p.fit Lat.-vel. map for l = 36.5 deg, b > +10 deg vb_434p.fit Lat.-vel. map for l = 37.0 deg, b > +10 deg vb_434n.fit Lat.-vel. map for l = 37.0 deg, b < -10 deg vb_435n.fit Lat.-vel. map for l = 37.5 deg, b < -10 deg vb_435p.fit Lat.-vel. map for l = 37.5 deg, b > +10 deg vb_436p.fit Lat.-vel. map for l = 38.0 deg, b > +10 deg vb_436n.fit Lat.-vel. map for l = 38.0 deg, b < -10 deg vb_437n.fit Lat.-vel. map for l = 38.5 deg, b < -10 deg vb_437p.fit Lat.-vel. map for l = 38.5 deg, b > +10 deg vb_438p.fit Lat.-vel. map for l = 39.0 deg, b > +10 deg vb_438n.fit Lat.-vel. map for l = 39.0 deg, b < -10 deg vb_439p.fit Lat.-vel. map for l = 39.5 deg, b > +10 deg vb_439n.fit Lat.-vel. map for l = 39.5 deg, b < -10 deg vb_440p.fit Lat.-vel. map for l = 40.0 deg, b > +10 deg vb_440n.fit Lat.-vel. map for l = 40.0 deg, b < -10 deg vb_441p.fit Lat.-vel. map for l = 40.5 deg, b > +10 deg vb_441n.fit Lat.-vel. map for l = 40.5 deg, b < -10 deg vb_442p.fit Lat.-vel. map for l = 41.0 deg, b > +10 deg vb_442n.fit Lat.-vel. map for l = 41.0 deg, b < -10 deg vb_443p.fit Lat.-vel. map for l = 41.5 deg, b > +10 deg vb_443n.fit Lat.-vel. map for l = 41.5 deg, b < -10 deg vb_444p.fit Lat.-vel. map for l = 42.0 deg, b > +10 deg vb_444n.fit Lat.-vel. map for l = 42.0 deg, b < -10 deg vb_445p.fit Lat.-vel. map for l = 42.5 deg, b > +10 deg vb_445n.fit Lat.-vel. map for l = 42.5 deg, b < -10 deg vb_446p.fit Lat.-vel. map for l = 43.0 deg, b > +10 deg vb_446n.fit Lat.-vel. map for l = 43.0 deg, b < -10 deg vb_447n.fit Lat.-vel. map for l = 43.5 deg, b < -10 deg vb_447p.fit Lat.-vel. map for l = 43.5 deg, b > +10 deg vb_448p.fit Lat.-vel. map for l = 44.0 deg, b > +10 deg vb_448n.fit Lat.-vel. map for l = 44.0 deg, b < -10 deg vb_449n.fit Lat.-vel. map for l = 44.5 deg, b < -10 deg vb_449p.fit Lat.-vel. map for l = 44.5 deg, b > +10 deg vb_450p.fit Lat.-vel. map for l = 45.0 deg, b > +10 deg vb_450n.fit Lat.-vel. map for l = 45.0 deg, b < -10 deg vb_451n.fit Lat.-vel. map for l = 45.5 deg, b < -10 deg vb_451p.fit Lat.-vel. map for l = 45.5 deg, b > +10 deg vb_452p.fit Lat.-vel. map for l = 46.0 deg, b > +10 deg vb_452n.fit Lat.-vel. map for l = 46.0 deg, b < -10 deg vb_453p.fit Lat.-vel. map for l = 46.5 deg, b > +10 deg vb_453n.fit Lat.-vel. map for l = 46.5 deg, b < -10 deg vb_454p.fit Lat.-vel. map for l = 47.0 deg, b > +10 deg vb_454n.fit Lat.-vel. map for l = 47.0 deg, b < -10 deg vb_455p.fit Lat.-vel. map for l = 47.5 deg, b > +10 deg vb_455n.fit Lat.-vel. map for l = 47.5 deg, b < -10 deg vb_456p.fit Lat.-vel. map for l = 48.0 deg, b > +10 deg vb_456n.fit Lat.-vel. map for l = 48.0 deg, b < -10 deg vb_457p.fit Lat.-vel. map for l = 48.5 deg, b > +10 deg vb_457n.fit Lat.-vel. map for l = 48.5 deg, b < -10 deg vb_458p.fit Lat.-vel. map for l = 49.0 deg, b > +10 deg vb_458n.fit Lat.-vel. map for l = 49.0 deg, b < -10 deg vb_459n.fit Lat.-vel. map for l = 49.5 deg, b < -10 deg vb_459p.fit Lat.-vel. map for l = 49.5 deg, b > +10 deg vb_460p.fit Lat.-vel. map for l = 50.0 deg, b > +10 deg vb_460n.fit Lat.-vel. map for l = 50.0 deg, b < -10 deg vb_461n.fit Lat.-vel. map for l = 50.5 deg, b < -10 deg vb_461p.fit Lat.-vel. map for l = 50.5 deg, b > +10 deg vb_462p.fit Lat.-vel. map for l = 51.0 deg, b > +10 deg vb_462n.fit Lat.-vel. map for l = 51.0 deg, b < -10 deg vb_463p.fit Lat.-vel. map for l = 51.5 deg, b > +10 deg vb_463n.fit Lat.-vel. map for l = 51.5 deg, b < -10 deg vb_464p.fit Lat.-vel. map for l = 52.0 deg, b > +10 deg vb_464n.fit Lat.-vel. map for l = 52.0 deg, b < -10 deg vb_465p.fit Lat.-vel. map for l = 52.5 deg, b > +10 deg vb_465n.fit Lat.-vel. map for l = 52.5 deg, b < -10 deg vb_466p.fit Lat.-vel. map for l = 53.0 deg, b > +10 deg vb_466n.fit Lat.-vel. map for l = 53.0 deg, b < -10 deg vb_467p.fit Lat.-vel. map for l = 53.5 deg, b > +10 deg vb_467n.fit Lat.-vel. map for l = 53.5 deg, b < -10 deg vb_468p.fit Lat.-vel. map for l = 54.0 deg, b > +10 deg vb_468n.fit Lat.-vel. map for l = 54.0 deg, b < -10 deg vb_469n.fit Lat.-vel. map for l = 54.5 deg, b < -10 deg vb_469p.fit Lat.-vel. map for l = 54.5 deg, b > +10 deg vb_470p.fit Lat.-vel. map for l = 55.0 deg, b > +10 deg vb_470n.fit Lat.-vel. map for l = 55.0 deg, b < -10 deg vb_471n.fit Lat.-vel. map for l = 55.5 deg, b < -10 deg vb_471p.fit Lat.-vel. map for l = 55.5 deg, b > +10 deg vb_472p.fit Lat.-vel. map for l = 56.0 deg, b > +10 deg vb_472n.fit Lat.-vel. map for l = 56.0 deg, b < -10 deg vb_473p.fit Lat.-vel. map for l = 56.5 deg, b > +10 deg vb_473n.fit Lat.-vel. map for l = 56.5 deg, b < -10 deg vb_474n.fit Lat.-vel. map for l = 57.0 deg, b < -10 deg vb_474p.fit Lat.-vel. map for l = 57.0 deg, b > +10 deg vb_475p.fit Lat.-vel. map for l = 57.5 deg, b > +10 deg vb_475n.fit Lat.-vel. map for l = 57.5 deg, b < -10 deg vb_476p.fit Lat.-vel. map for l = 58.0 deg, b > +10 deg vb_476n.fit Lat.-vel. map for l = 58.0 deg, b < -10 deg vb_477p.fit Lat.-vel. map for l = 58.5 deg, b > +10 deg vb_477n.fit Lat.-vel. map for l = 58.5 deg, b < -10 deg vb_478p.fit Lat.-vel. map for l = 59.0 deg, b > +10 deg vb_478n.fit Lat.-vel. map for l = 59.0 deg, b < -10 deg vb_479p.fit Lat.-vel. map for l = 59.5 deg, b > +10 deg vb_479n.fit Lat.-vel. map for l = 59.5 deg, b < -10 deg vb_480p.fit Lat.-vel. map for l = 60.0 deg, b > +10 deg vb_480n.fit Lat.-vel. map for l = 60.0 deg, b < -10 deg vb_481p.fit Lat.-vel. map for l = 60.5 deg, b > +10 deg vb_481n.fit Lat.-vel. map for l = 60.5 deg, b < -10 deg vb_482p.fit Lat.-vel. map for l = 61.0 deg, b > +10 deg vb_482n.fit Lat.-vel. map for l = 61.0 deg, b < -10 deg vb_483p.fit Lat.-vel. map for l = 61.5 deg, b > +10 deg vb_483n.fit Lat.-vel. map for l = 61.5 deg, b < -10 deg vb_484p.fit Lat.-vel. map for l = 62.0 deg, b > +10 deg vb_484n.fit Lat.-vel. map for l = 62.0 deg, b < -10 deg vb_485p.fit Lat.-vel. map for l = 62.5 deg, b > +10 deg vb_485n.fit Lat.-vel. map for l = 62.5 deg, b < -10 deg vb_486p.fit Lat.-vel. map for l = 63.0 deg, b > +10 deg vb_486n.fit Lat.-vel. map for l = 63.0 deg, b < -10 deg vb_487p.fit Lat.-vel. map for l = 63.5 deg, b > +10 deg vb_487n.fit Lat.-vel. map for l = 63.5 deg, b < -10 deg vb_488p.fit Lat.-vel. map for l = 64.0 deg, b > +10 deg vb_488n.fit Lat.-vel. map for l = 64.0 deg, b < -10 deg vb_489p.fit Lat.-vel. map for l = 64.5 deg, b > +10 deg vb_489n.fit Lat.-vel. map for l = 64.5 deg, b < -10 deg vb_490p.fit Lat.-vel. map for l = 65.0 deg, b > +10 deg vb_490n.fit Lat.-vel. map for l = 65.0 deg, b < -10 deg vb_491p.fit Lat.-vel. map for l = 65.5 deg, b > +10 deg vb_491n.fit Lat.-vel. map for l = 65.5 deg, b < -10 deg vb_492p.fit Lat.-vel. map for l = 66.0 deg, b > +10 deg vb_492n.fit Lat.-vel. map for l = 66.0 deg, b < -10 deg vb_493p.fit Lat.-vel. map for l = 66.5 deg, b > +10 deg vb_493n.fit Lat.-vel. map for l = 66.5 deg, b < -10 deg vb_494p.fit Lat.-vel. map for l = 67.0 deg, b > +10 deg vb_494n.fit Lat.-vel. map for l = 67.0 deg, b < -10 deg vb_495p.fit Lat.-vel. map for l = 67.5 deg, b > +10 deg vb_495n.fit Lat.-vel. map for l = 67.5 deg, b < -10 deg vb_496p.fit Lat.-vel. map for l = 68.0 deg, b > +10 deg vb_496n.fit Lat.-vel. map for l = 68.0 deg, b < -10 deg vb_497p.fit Lat.-vel. map for l = 68.5 deg, b > +10 deg vb_497n.fit Lat.-vel. map for l = 68.5 deg, b < -10 deg vb_498p.fit Lat.-vel. map for l = 69.0 deg, b > +10 deg vb_498n.fit Lat.-vel. map for l = 69.0 deg, b < -10 deg vb_499p.fit Lat.-vel. map for l = 69.5 deg, b > +10 deg vb_499n.fit Lat.-vel. map for l = 69.5 deg, b < -10 deg vb_500p.fit Lat.-vel. map for l = 70.0 deg, b > +10 deg vb_500n.fit Lat.-vel. map for l = 70.0 deg, b < -10 deg vb_501p.fit Lat.-vel. map for l = 70.5 deg, b > +10 deg vb_501n.fit Lat.-vel. map for l = 70.5 deg, b < -10 deg vb_502p.fit Lat.-vel. map for l = 71.0 deg, b > +10 deg vb_502n.fit Lat.-vel. map for l = 71.0 deg, b < -10 deg vb_503n.fit Lat.-vel. map for l = 71.5 deg, b < -10 deg vb_503p.fit Lat.-vel. map for l = 71.5 deg, b > +10 deg vb_504p.fit Lat.-vel. map for l = 72.0 deg, b > +10 deg vb_504n.fit Lat.-vel. map for l = 72.0 deg, b < -10 deg vb_505n.fit Lat.-vel. map for l = 72.5 deg, b < -10 deg vb_505p.fit Lat.-vel. map for l = 72.5 deg, b > +10 deg vb_506p.fit Lat.-vel. map for l = 73.0 deg, b > +10 deg vb_506n.fit Lat.-vel. map for l = 73.0 deg, b < -10 deg vb_507n.fit Lat.-vel. map for l = 73.5 deg, b < -10 deg vb_507p.fit Lat.-vel. map for l = 73.5 deg, b > +10 deg vb_508p.fit Lat.-vel. map for l = 74.0 deg, b > +10 deg vb_508n.fit Lat.-vel. map for l = 74.0 deg, b < -10 deg vb_509n.fit Lat.-vel. map for l = 74.5 deg, b < -10 deg vb_509p.fit Lat.-vel. map for l = 74.5 deg, b > +10 deg vb_510p.fit Lat.-vel. map for l = 75.0 deg, b > +10 deg vb_510n.fit Lat.-vel. map for l = 75.0 deg, b < -10 deg vb_511n.fit Lat.-vel. map for l = 75.5 deg, b < -10 deg vb_511p.fit Lat.-vel. map for l = 75.5 deg, b > +10 deg vb_512p.fit Lat.-vel. map for l = 76.0 deg, b > +10 deg vb_512n.fit Lat.-vel. map for l = 76.0 deg, b < -10 deg vb_513n.fit Lat.-vel. map for l = 76.5 deg, b < -10 deg vb_513p.fit Lat.-vel. map for l = 76.5 deg, b > +10 deg vb_514p.fit Lat.-vel. map for l = 77.0 deg, b > +10 deg vb_514n.fit Lat.-vel. map for l = 77.0 deg, b < -10 deg vb_515n.fit Lat.-vel. map for l = 77.5 deg, b < -10 deg vb_515p.fit Lat.-vel. map for l = 77.5 deg, b > +10 deg vb_516p.fit Lat.-vel. map for l = 78.0 deg, b > +10 deg vb_516n.fit Lat.-vel. map for l = 78.0 deg, b < -10 deg vb_517n.fit Lat.-vel. map for l = 78.5 deg, b < -10 deg vb_517p.fit Lat.-vel. map for l = 78.5 deg, b > +10 deg vb_518p.fit Lat.-vel. map for l = 79.0 deg, b > +10 deg vb_518n.fit Lat.-vel. map for l = 79.0 deg, b < -10 deg vb_519n.fit Lat.-vel. map for l = 79.5 deg, b < -10 deg vb_519p.fit Lat.-vel. map for l = 79.5 deg, b > +10 deg vb_520p.fit Lat.-vel. map for l = 80.0 deg, b > +10 deg vb_520n.fit Lat.-vel. map for l = 80.0 deg, b < -10 deg vb_521p.fit Lat.-vel. map for l = 80.5 deg, b > +10 deg vb_521n.fit Lat.-vel. map for l = 80.5 deg, b < -10 deg vb_522p.fit Lat.-vel. map for l = 81.0 deg, b > +10 deg vb_522n.fit Lat.-vel. map for l = 81.0 deg, b < -10 deg vb_523n.fit Lat.-vel. map for l = 81.5 deg, b < -10 deg vb_523p.fit Lat.-vel. map for l = 81.5 deg, b > +10 deg vb_524p.fit Lat.-vel. map for l = 82.0 deg, b > +10 deg vb_524n.fit Lat.-vel. map for l = 82.0 deg, b < -10 deg vb_525n.fit Lat.-vel. map for l = 82.5 deg, b < -10 deg vb_525p.fit Lat.-vel. map for l = 82.5 deg, b > +10 deg vb_526p.fit Lat.-vel. map for l = 83.0 deg, b > +10 deg vb_526n.fit Lat.-vel. map for l = 83.0 deg, b < -10 deg vb_527n.fit Lat.-vel. map for l = 83.5 deg, b < -10 deg vb_527p.fit Lat.-vel. map for l = 83.5 deg, b > +10 deg vb_528p.fit Lat.-vel. map for l = 84.0 deg, b > +10 deg vb_528n.fit Lat.-vel. map for l = 84.0 deg, b < -10 deg vb_529n.fit Lat.-vel. map for l = 84.5 deg, b < -10 deg vb_529p.fit Lat.-vel. map for l = 84.5 deg, b > +10 deg vb_530p.fit Lat.-vel. map for l = 85.0 deg, b > +10 deg vb_530n.fit Lat.-vel. map for l = 85.0 deg, b < -10 deg vb_531n.fit Lat.-vel. map for l = 85.5 deg, b < -10 deg vb_531p.fit Lat.-vel. map for l = 85.5 deg, b > +10 deg vb_532p.fit Lat.-vel. map for l = 86.0 deg, b > +10 deg vb_532n.fit Lat.-vel. map for l = 86.0 deg, b < -10 deg vb_533p.fit Lat.-vel. map for l = 86.5 deg, b > +10 deg vb_533n.fit Lat.-vel. map for l = 86.5 deg, b < -10 deg vb_534p.fit Lat.-vel. map for l = 87.0 deg, b > +10 deg vb_534n.fit Lat.-vel. map for l = 87.0 deg, b < -10 deg vb_535n.fit Lat.-vel. map for l = 87.5 deg, b < -10 deg vb_535p.fit Lat.-vel. map for l = 87.5 deg, b > +10 deg vb_536p.fit Lat.-vel. map for l = 88.0 deg, b > +10 deg vb_536n.fit Lat.-vel. map for l = 88.0 deg, b < -10 deg vb_537n.fit Lat.-vel. map for l = 88.5 deg, b < -10 deg vb_537p.fit Lat.-vel. map for l = 88.5 deg, b > +10 deg vb_538p.fit Lat.-vel. map for l = 89.0 deg, b > +10 deg vb_538n.fit Lat.-vel. map for l = 89.0 deg, b < -10 deg vb_539n.fit Lat.-vel. map for l = 89.5 deg, b < -10 deg vb_539p.fit Lat.-vel. map for l = 89.5 deg, b > +10 deg vb_540p.fit Lat.-vel. map for l = 90.0 deg, b > +10 deg vb_540n.fit Lat.-vel. map for l = 90.0 deg, b < -10 deg vb_541n.fit Lat.-vel. map for l = 90.5 deg, b < -10 deg vb_541p.fit Lat.-vel. map for l = 90.5 deg, b > +10 deg vb_542p.fit Lat.-vel. map for l = 91.0 deg, b > +10 deg vb_542n.fit Lat.-vel. map for l = 91.0 deg, b < -10 deg vb_543n.fit Lat.-vel. map for l = 91.5 deg, b < -10 deg vb_543p.fit Lat.-vel. map for l = 91.5 deg, b > +10 deg vb_544p.fit Lat.-vel. map for l = 92.0 deg, b > +10 deg vb_544n.fit Lat.-vel. map for l = 92.0 deg, b < -10 deg vb_545p.fit Lat.-vel. map for l = 92.5 deg, b > +10 deg vb_545n.fit Lat.-vel. map for l = 92.5 deg, b < -10 deg vb_546p.fit Lat.-vel. map for l = 93.0 deg, b > +10 deg vb_546n.fit Lat.-vel. map for l = 93.0 deg, b < -10 deg vb_547n.fit Lat.-vel. map for l = 93.5 deg, b < -10 deg vb_547p.fit Lat.-vel. map for l = 93.5 deg, b > +10 deg vb_548p.fit Lat.-vel. map for l = 94.0 deg, b > +10 deg vb_548n.fit Lat.-vel. map for l = 94.0 deg, b < -10 deg vb_549n.fit Lat.-vel. map for l = 94.5 deg, b < -10 deg vb_549p.fit Lat.-vel. map for l = 94.5 deg, b > +10 deg vb_550p.fit Lat.-vel. map for l = 95.0 deg, b > +10 deg vb_550n.fit Lat.-vel. map for l = 95.0 deg, b < -10 deg vb_551n.fit Lat.-vel. map for l = 95.5 deg, b < -10 deg vb_551p.fit Lat.-vel. map for l = 95.5 deg, b > +10 deg vb_552p.fit Lat.-vel. map for l = 96.0 deg, b > +10 deg vb_552n.fit Lat.-vel. map for l = 96.0 deg, b < -10 deg vb_553n.fit Lat.-vel. map for l = 96.5 deg, b < -10 deg vb_553p.fit Lat.-vel. map for l = 96.5 deg, b > +10 deg vb_554p.fit Lat.-vel. map for l = 97.0 deg, b > +10 deg vb_554n.fit Lat.-vel. map for l = 97.0 deg, b < -10 deg vb_555n.fit Lat.-vel. map for l = 97.5 deg, b < -10 deg vb_555p.fit Lat.-vel. map for l = 97.5 deg, b > +10 deg vb_556p.fit Lat.-vel. map for l = 98.0 deg, b > +10 deg vb_556n.fit Lat.-vel. map for l = 98.0 deg, b < -10 deg vb_557p.fit Lat.-vel. map for l = 98.5 deg, b > +10 deg vb_557n.fit Lat.-vel. map for l = 98.5 deg, b < -10 deg vb_558p.fit Lat.-vel. map for l = 99.0 deg, b > +10 deg vb_558n.fit Lat.-vel. map for l = 99.0 deg, b < -10 deg vb_559n.fit Lat.-vel. map for l = 99.5 deg, b < -10 deg vb_559p.fit Lat.-vel. map for l = 99.5 deg, b > +10 deg vb_560p.fit Lat.-vel. map for l = 100.0 deg, b > +10 deg vb_560n.fit Lat.-vel. map for l = 100.0 deg, b < -10 deg vb_561n.fit Lat.-vel. map for l = 100.5 deg, b < -10 deg vb_561p.fit Lat.-vel. map for l = 100.5 deg, b > +10 deg vb_562p.fit Lat.-vel. map for l = 101.0 deg, b > +10 deg vb_562n.fit Lat.-vel. map for l = 101.0 deg, b < -10 deg vb_563n.fit Lat.-vel. map for l = 101.5 deg, b < -10 deg vb_563p.fit Lat.-vel. map for l = 101.5 deg, b > +10 deg vb_564p.fit Lat.-vel. map for l = 102.0 deg, b > +10 deg vb_564n.fit Lat.-vel. map for l = 102.0 deg, b < -10 deg vb_565n.fit Lat.-vel. map for l = 102.5 deg, b < -10 deg vb_565p.fit Lat.-vel. map for l = 102.5 deg, b > +10 deg vb_566p.fit Lat.-vel. map for l = 103.0 deg, b > +10 deg vb_566n.fit Lat.-vel. map for l = 103.0 deg, b < -10 deg vb_567p.fit Lat.-vel. map for l = 103.5 deg, b > +10 deg vb_567n.fit Lat.-vel. map for l = 103.5 deg, b < -10 deg vb_568n.fit Lat.-vel. map for l = 104.0 deg, b < -10 deg vb_568p.fit Lat.-vel. map for l = 104.0 deg, b > +10 deg vb_569n.fit Lat.-vel. map for l = 104.5 deg, b < -10 deg vb_569p.fit Lat.-vel. map for l = 104.5 deg, b > +10 deg vb_570p.fit Lat.-vel. map for l = 105.0 deg, b > +10 deg vb_570n.fit Lat.-vel. map for l = 105.0 deg, b < -10 deg vb_571n.fit Lat.-vel. map for l = 105.5 deg, b < -10 deg vb_571p.fit Lat.-vel. map for l = 105.5 deg, b > +10 deg vb_572p.fit Lat.-vel. map for l = 106.0 deg, b > +10 deg vb_572n.fit Lat.-vel. map for l = 106.0 deg, b < -10 deg vb_573n.fit Lat.-vel. map for l = 106.5 deg, b < -10 deg vb_573p.fit Lat.-vel. map for l = 106.5 deg, b > +10 deg vb_574p.fit Lat.-vel. map for l = 107.0 deg, b > +10 deg vb_574n.fit Lat.-vel. map for l = 107.0 deg, b < -10 deg vb_575n.fit Lat.-vel. map for l = 107.5 deg, b < -10 deg vb_575p.fit Lat.-vel. map for l = 107.5 deg, b > +10 deg vb_576p.fit Lat.-vel. map for l = 108.0 deg, b > +10 deg vb_576n.fit Lat.-vel. map for l = 108.0 deg, b < -10 deg vb_577p.fit Lat.-vel. map for l = 108.5 deg, b > +10 deg vb_577n.fit Lat.-vel. map for l = 108.5 deg, b < -10 deg vb_578p.fit Lat.-vel. map for l = 109.0 deg, b > +10 deg vb_578n.fit Lat.-vel. map for l = 109.0 deg, b < -10 deg vb_579p.fit Lat.-vel. map for l = 109.5 deg, b > +10 deg vb_579n.fit Lat.-vel. map for l = 109.5 deg, b < -10 deg vb_580p.fit Lat.-vel. map for l = 110.0 deg, b > +10 deg vb_580n.fit Lat.-vel. map for l = 110.0 deg, b < -10 deg vb_581n.fit Lat.-vel. map for l = 110.5 deg, b < -10 deg vb_581p.fit Lat.-vel. map for l = 110.5 deg, b > +10 deg vb_582p.fit Lat.-vel. map for l = 111.0 deg, b > +10 deg vb_582n.fit Lat.-vel. map for l = 111.0 deg, b < -10 deg vb_583n.fit Lat.-vel. map for l = 111.5 deg, b < -10 deg vb_583p.fit Lat.-vel. map for l = 111.5 deg, b > +10 deg vb_584p.fit Lat.-vel. map for l = 112.0 deg, b > +10 deg vb_584n.fit Lat.-vel. map for l = 112.0 deg, b < -10 deg vb_585n.fit Lat.-vel. map for l = 112.5 deg, b < -10 deg vb_585p.fit Lat.-vel. map for l = 112.5 deg, b > +10 deg vb_586p.fit Lat.-vel. map for l = 113.0 deg, b > +10 deg vb_586n.fit Lat.-vel. map for l = 113.0 deg, b < -10 deg vb_587p.fit Lat.-vel. map for l = 113.5 deg, b > +10 deg vb_587n.fit Lat.-vel. map for l = 113.5 deg, b < -10 deg vb_588p.fit Lat.-vel. map for l = 114.0 deg, b > +10 deg vb_588n.fit Lat.-vel. map for l = 114.0 deg, b < -10 deg vb_589p.fit Lat.-vel. map for l = 114.5 deg, b > +10 deg vb_589n.fit Lat.-vel. map for l = 114.5 deg, b < -10 deg vb_590p.fit Lat.-vel. map for l = 115.0 deg, b > +10 deg vb_590n.fit Lat.-vel. map for l = 115.0 deg, b < -10 deg vb_591p.fit Lat.-vel. map for l = 115.5 deg, b > +10 deg vb_591n.fit Lat.-vel. map for l = 115.5 deg, b < -10 deg vb_592p.fit Lat.-vel. map for l = 116.0 deg, b > +10 deg vb_592n.fit Lat.-vel. map for l = 116.0 deg, b < -10 deg vb_593n.fit Lat.-vel. map for l = 116.5 deg, b < -10 deg vb_593p.fit Lat.-vel. map for l = 116.5 deg, b > +10 deg vb_594p.fit Lat.-vel. map for l = 117.0 deg, b > +10 deg vb_594n.fit Lat.-vel. map for l = 117.0 deg, b < -10 deg vb_595n.fit Lat.-vel. map for l = 117.5 deg, b < -10 deg vb_595p.fit Lat.-vel. map for l = 117.5 deg, b > +10 deg vb_596p.fit Lat.-vel. map for l = 118.0 deg, b > +10 deg vb_596n.fit Lat.-vel. map for l = 118.0 deg, b < -10 deg vb_597n.fit Lat.-vel. map for l = 118.5 deg, b < -10 deg vb_597p.fit Lat.-vel. map for l = 118.5 deg, b > +10 deg vb_598p.fit Lat.-vel. map for l = 119.0 deg, b > +10 deg vb_598n.fit Lat.-vel. map for l = 119.0 deg, b < -10 deg vb_599p.fit Lat.-vel. map for l = 119.5 deg, b > +10 deg vb_599n.fit Lat.-vel. map for l = 119.5 deg, b < -10 deg vb_600p.fit Lat.-vel. map for l = 120.0 deg, b > +10 deg vb_600n.fit Lat.-vel. map for l = 120.0 deg, b < -10 deg vb_601p.fit Lat.-vel. map for l = 120.5 deg, b > +10 deg vb_601n.fit Lat.-vel. map for l = 120.5 deg, b < -10 deg vb_602p.fit Lat.-vel. map for l = 121.0 deg, b > +10 deg vb_602n.fit Lat.-vel. map for l = 121.0 deg, b < -10 deg vb_603p.fit Lat.-vel. map for l = 121.5 deg, b > +10 deg vb_603n.fit Lat.-vel. map for l = 121.5 deg, b < -10 deg vb_604p.fit Lat.-vel. map for l = 122.0 deg, b > +10 deg vb_604n.fit Lat.-vel. map for l = 122.0 deg, b < -10 deg vb_605p.fit Lat.-vel. map for l = 122.5 deg, b > +10 deg vb_605n.fit Lat.-vel. map for l = 122.5 deg, b < -10 deg vb_606p.fit Lat.-vel. map for l = 123.0 deg, b > +10 deg vb_606n.fit Lat.-vel. map for l = 123.0 deg, b < -10 deg vb_607p.fit Lat.-vel. map for l = 123.5 deg, b > +10 deg vb_607n.fit Lat.-vel. map for l = 123.5 deg, b < -10 deg vb_608p.fit Lat.-vel. map for l = 124.0 deg, b > +10 deg vb_608n.fit Lat.-vel. map for l = 124.0 deg, b < -10 deg vb_609p.fit Lat.-vel. map for l = 124.5 deg, b > +10 deg vb_609n.fit Lat.-vel. map for l = 124.5 deg, b < -10 deg vb_610p.fit Lat.-vel. map for l = 125.0 deg, b > +10 deg vb_610n.fit Lat.-vel. map for l = 125.0 deg, b < -10 deg vb_611n.fit Lat.-vel. map for l = 125.5 deg, b < -10 deg vb_611p.fit Lat.-vel. map for l = 125.5 deg, b > +10 deg vb_612p.fit Lat.-vel. map for l = 126.0 deg, b > +10 deg vb_612n.fit Lat.-vel. map for l = 126.0 deg, b < -10 deg vb_613n.fit Lat.-vel. map for l = 126.5 deg, b < -10 deg vb_613p.fit Lat.-vel. map for l = 126.5 deg, b > +10 deg vb_614p.fit Lat.-vel. map for l = 127.0 deg, b > +10 deg vb_614n.fit Lat.-vel. map for l = 127.0 deg, b < -10 deg vb_615p.fit Lat.-vel. map for l = 127.5 deg, b > +10 deg vb_615n.fit Lat.-vel. map for l = 127.5 deg, b < -10 deg vb_616p.fit Lat.-vel. map for l = 128.0 deg, b > +10 deg vb_616n.fit Lat.-vel. map for l = 128.0 deg, b < -10 deg vb_617n.fit Lat.-vel. map for l = 128.5 deg, b < -10 deg vb_617p.fit Lat.-vel. map for l = 128.5 deg, b > +10 deg vb_618p.fit Lat.-vel. map for l = 129.0 deg, b > +10 deg vb_618n.fit Lat.-vel. map for l = 129.0 deg, b < -10 deg vb_619n.fit Lat.-vel. map for l = 129.5 deg, b < -10 deg vb_619p.fit Lat.-vel. map for l = 129.5 deg, b > +10 deg vb_620p.fit Lat.-vel. map for l = 130.0 deg, b > +10 deg vb_620n.fit Lat.-vel. map for l = 130.0 deg, b < -10 deg vb_621n.fit Lat.-vel. map for l = 130.5 deg, b < -10 deg vb_621p.fit Lat.-vel. map for l = 130.5 deg, b > +10 deg vb_622p.fit Lat.-vel. map for l = 131.0 deg, b > +10 deg vb_622n.fit Lat.-vel. map for l = 131.0 deg, b < -10 deg vb_623n.fit Lat.-vel. map for l = 131.5 deg, b < -10 deg vb_623p.fit Lat.-vel. map for l = 131.5 deg, b > +10 deg vb_624p.fit Lat.-vel. map for l = 132.0 deg, b > +10 deg vb_624n.fit Lat.-vel. map for l = 132.0 deg, b < -10 deg vb_625n.fit Lat.-vel. map for l = 132.5 deg, b < -10 deg vb_625p.fit Lat.-vel. map for l = 132.5 deg, b > +10 deg vb_626p.fit Lat.-vel. map for l = 133.0 deg, b > +10 deg vb_626n.fit Lat.-vel. map for l = 133.0 deg, b < -10 deg vb_627p.fit Lat.-vel. map for l = 133.5 deg, b > +10 deg vb_627n.fit Lat.-vel. map for l = 133.5 deg, b < -10 deg vb_628p.fit Lat.-vel. map for l = 134.0 deg, b > +10 deg vb_628n.fit Lat.-vel. map for l = 134.0 deg, b < -10 deg vb_629p.fit Lat.-vel. map for l = 134.5 deg, b > +10 deg vb_629n.fit Lat.-vel. map for l = 134.5 deg, b < -10 deg vb_630p.fit Lat.-vel. map for l = 135.0 deg, b > +10 deg vb_630n.fit Lat.-vel. map for l = 135.0 deg, b < -10 deg vb_631p.fit Lat.-vel. map for l = 135.5 deg, b > +10 deg vb_631n.fit Lat.-vel. map for l = 135.5 deg, b < -10 deg vb_632p.fit Lat.-vel. map for l = 136.0 deg, b > +10 deg vb_632n.fit Lat.-vel. map for l = 136.0 deg, b < -10 deg vb_633n.fit Lat.-vel. map for l = 136.5 deg, b < -10 deg vb_633p.fit Lat.-vel. map for l = 136.5 deg, b > +10 deg vb_634p.fit Lat.-vel. map for l = 137.0 deg, b > +10 deg vb_634n.fit Lat.-vel. map for l = 137.0 deg, b < -10 deg vb_635n.fit Lat.-vel. map for l = 137.5 deg, b < -10 deg vb_635p.fit Lat.-vel. map for l = 137.5 deg, b > +10 deg vb_636p.fit Lat.-vel. map for l = 138.0 deg, b > +10 deg vb_636n.fit Lat.-vel. map for l = 138.0 deg, b < -10 deg vb_637n.fit Lat.-vel. map for l = 138.5 deg, b < -10 deg vb_637p.fit Lat.-vel. map for l = 138.5 deg, b > +10 deg vb_638p.fit Lat.-vel. map for l = 139.0 deg, b > +10 deg vb_638n.fit Lat.-vel. map for l = 139.0 deg, b < -10 deg vb_639n.fit Lat.-vel. map for l = 139.5 deg, b < -10 deg vb_639p.fit Lat.-vel. map for l = 139.5 deg, b > +10 deg vb_640p.fit Lat.-vel. map for l = 140.0 deg, b > +10 deg vb_640n.fit Lat.-vel. map for l = 140.0 deg, b < -10 deg vb_641p.fit Lat.-vel. map for l = 140.5 deg, b > +10 deg vb_641n.fit Lat.-vel. map for l = 140.5 deg, b < -10 deg vb_642p.fit Lat.-vel. map for l = 141.0 deg, b > +10 deg vb_642n.fit Lat.-vel. map for l = 141.0 deg, b < -10 deg vb_643p.fit Lat.-vel. map for l = 141.5 deg, b > +10 deg vb_643n.fit Lat.-vel. map for l = 141.5 deg, b < -10 deg vb_644p.fit Lat.-vel. map for l = 142.0 deg, b > +10 deg vb_644n.fit Lat.-vel. map for l = 142.0 deg, b < -10 deg vb_645p.fit Lat.-vel. map for l = 142.5 deg, b > +10 deg vb_645n.fit Lat.-vel. map for l = 142.5 deg, b < -10 deg vb_646p.fit Lat.-vel. map for l = 143.0 deg, b > +10 deg vb_646n.fit Lat.-vel. map for l = 143.0 deg, b < -10 deg vb_647n.fit Lat.-vel. map for l = 143.5 deg, b < -10 deg vb_647p.fit Lat.-vel. map for l = 143.5 deg, b > +10 deg vb_648p.fit Lat.-vel. map for l = 144.0 deg, b > +10 deg vb_648n.fit Lat.-vel. map for l = 144.0 deg, b < -10 deg vb_649p.fit Lat.-vel. map for l = 144.5 deg, b > +10 deg vb_649n.fit Lat.-vel. map for l = 144.5 deg, b < -10 deg vb_650p.fit Lat.-vel. map for l = 145.0 deg, b > +10 deg vb_650n.fit Lat.-vel. map for l = 145.0 deg, b < -10 deg vb_651p.fit Lat.-vel. map for l = 145.5 deg, b > +10 deg vb_651n.fit Lat.-vel. map for l = 145.5 deg, b < -10 deg vb_652p.fit Lat.-vel. map for l = 146.0 deg, b > +10 deg vb_652n.fit Lat.-vel. map for l = 146.0 deg, b < -10 deg vb_653p.fit Lat.-vel. map for l = 146.5 deg, b > +10 deg vb_653n.fit Lat.-vel. map for l = 146.5 deg, b < -10 deg vb_654p.fit Lat.-vel. map for l = 147.0 deg, b > +10 deg vb_654n.fit Lat.-vel. map for l = 147.0 deg, b < -10 deg vb_655n.fit Lat.-vel. map for l = 147.5 deg, b < -10 deg vb_655p.fit Lat.-vel. map for l = 147.5 deg, b > +10 deg vb_656p.fit Lat.-vel. map for l = 148.0 deg, b > +10 deg vb_656n.fit Lat.-vel. map for l = 148.0 deg, b < -10 deg vb_657p.fit Lat.-vel. map for l = 148.5 deg, b > +10 deg vb_657n.fit Lat.-vel. map for l = 148.5 deg, b < -10 deg vb_658p.fit Lat.-vel. map for l = 149.0 deg, b > +10 deg vb_658n.fit Lat.-vel. map for l = 149.0 deg, b < -10 deg vb_659n.fit Lat.-vel. map for l = 149.5 deg, b < -10 deg vb_659p.fit Lat.-vel. map for l = 149.5 deg, b > +10 deg vb_660p.fit Lat.-vel. map for l = 150.0 deg, b > +10 deg vb_660n.fit Lat.-vel. map for l = 150.0 deg, b < -10 deg vb_661p.fit Lat.-vel. map for l = 150.5 deg, b > +10 deg vb_661n.fit Lat.-vel. map for l = 150.5 deg, b < -10 deg vb_662p.fit Lat.-vel. map for l = 151.0 deg, b > +10 deg vb_662n.fit Lat.-vel. map for l = 151.0 deg, b < -10 deg vb_663p.fit Lat.-vel. map for l = 151.5 deg, b > +10 deg vb_663n.fit Lat.-vel. map for l = 151.5 deg, b < -10 deg vb_664p.fit Lat.-vel. map for l = 152.0 deg, b > +10 deg vb_664n.fit Lat.-vel. map for l = 152.0 deg, b < -10 deg vb_665p.fit Lat.-vel. map for l = 152.5 deg, b > +10 deg vb_665n.fit Lat.-vel. map for l = 152.5 deg, b < -10 deg vb_666p.fit Lat.-vel. map for l = 153.0 deg, b > +10 deg vb_666n.fit Lat.-vel. map for l = 153.0 deg, b < -10 deg vb_667p.fit Lat.-vel. map for l = 153.5 deg, b > +10 deg vb_667n.fit Lat.-vel. map for l = 153.5 deg, b < -10 deg vb_668p.fit Lat.-vel. map for l = 154.0 deg, b > +10 deg vb_668n.fit Lat.-vel. map for l = 154.0 deg, b < -10 deg vb_669n.fit Lat.-vel. map for l = 154.5 deg, b < -10 deg vb_669p.fit Lat.-vel. map for l = 154.5 deg, b > +10 deg vb_670p.fit Lat.-vel. map for l = 155.0 deg, b > +10 deg vb_670n.fit Lat.-vel. map for l = 155.0 deg, b < -10 deg vb_671p.fit Lat.-vel. map for l = 155.5 deg, b > +10 deg vb_671n.fit Lat.-vel. map for l = 155.5 deg, b < -10 deg vb_672p.fit Lat.-vel. map for l = 156.0 deg, b > +10 deg vb_672n.fit Lat.-vel. map for l = 156.0 deg, b < -10 deg vb_673p.fit Lat.-vel. map for l = 156.5 deg, b > +10 deg vb_673n.fit Lat.-vel. map for l = 156.5 deg, b < -10 deg vb_674n.fit Lat.-vel. map for l = 157.0 deg, b < -10 deg vb_674p.fit Lat.-vel. map for l = 157.0 deg, b > +10 deg vb_675n.fit Lat.-vel. map for l = 157.5 deg, b < -10 deg vb_675p.fit Lat.-vel. map for l = 157.5 deg, b > +10 deg vb_676p.fit Lat.-vel. map for l = 158.0 deg, b > +10 deg vb_676n.fit Lat.-vel. map for l = 158.0 deg, b < -10 deg vb_677p.fit Lat.-vel. map for l = 158.5 deg, b > +10 deg vb_677n.fit Lat.-vel. map for l = 158.5 deg, b < -10 deg vb_678p.fit Lat.-vel. map for l = 159.0 deg, b > +10 deg vb_678n.fit Lat.-vel. map for l = 159.0 deg, b < -10 deg vb_679n.fit Lat.-vel. map for l = 159.5 deg, b < -10 deg vb_679p.fit Lat.-vel. map for l = 159.5 deg, b > +10 deg vb_680p.fit Lat.-vel. map for l = 160.0 deg, b > +10 deg vb_680n.fit Lat.-vel. map for l = 160.0 deg, b < -10 deg vb_681n.fit Lat.-vel. map for l = 160.5 deg, b < -10 deg vb_681p.fit Lat.-vel. map for l = 160.5 deg, b > +10 deg vb_682p.fit Lat.-vel. map for l = 161.0 deg, b > +10 deg vb_682n.fit Lat.-vel. map for l = 161.0 deg, b < -10 deg vb_683n.fit Lat.-vel. map for l = 161.5 deg, b < -10 deg vb_683p.fit Lat.-vel. map for l = 161.5 deg, b > +10 deg vb_684p.fit Lat.-vel. map for l = 162.0 deg, b > +10 deg vb_684n.fit Lat.-vel. map for l = 162.0 deg, b < -10 deg vb_685p.fit Lat.-vel. map for l = 162.5 deg, b > +10 deg vb_685n.fit Lat.-vel. map for l = 162.5 deg, b < -10 deg vb_686p.fit Lat.-vel. map for l = 163.0 deg, b > +10 deg vb_686n.fit Lat.-vel. map for l = 163.0 deg, b < -10 deg vb_687n.fit Lat.-vel. map for l = 163.5 deg, b < -10 deg vb_687p.fit Lat.-vel. map for l = 163.5 deg, b > +10 deg vb_688p.fit Lat.-vel. map for l = 164.0 deg, b > +10 deg vb_688n.fit Lat.-vel. map for l = 164.0 deg, b < -10 deg vb_689p.fit Lat.-vel. map for l = 164.5 deg, b > +10 deg vb_689n.fit Lat.-vel. map for l = 164.5 deg, b < -10 deg vb_690p.fit Lat.-vel. map for l = 165.0 deg, b > +10 deg vb_690n.fit Lat.-vel. map for l = 165.0 deg, b < -10 deg vb_691n.fit Lat.-vel. map for l = 165.5 deg, b < -10 deg vb_691p.fit Lat.-vel. map for l = 165.5 deg, b > +10 deg vb_692p.fit Lat.-vel. map for l = 166.0 deg, b > +10 deg vb_692n.fit Lat.-vel. map for l = 166.0 deg, b < -10 deg vb_693n.fit Lat.-vel. map for l = 166.5 deg, b < -10 deg vb_693p.fit Lat.-vel. map for l = 166.5 deg, b > +10 deg vb_694p.fit Lat.-vel. map for l = 167.0 deg, b > +10 deg vb_694n.fit Lat.-vel. map for l = 167.0 deg, b < -10 deg vb_695n.fit Lat.-vel. map for l = 167.5 deg, b < -10 deg vb_695p.fit Lat.-vel. map for l = 167.5 deg, b > +10 deg vb_696p.fit Lat.-vel. map for l = 168.0 deg, b > +10 deg vb_696n.fit Lat.-vel. map for l = 168.0 deg, b < -10 deg vb_697n.fit Lat.-vel. map for l = 168.5 deg, b < -10 deg vb_697p.fit Lat.-vel. map for l = 168.5 deg, b > +10 deg vb_698p.fit Lat.-vel. map for l = 169.0 deg, b > +10 deg vb_698n.fit Lat.-vel. map for l = 169.0 deg, b < -10 deg vb_699p.fit Lat.-vel. map for l = 169.5 deg, b > +10 deg vb_699n.fit Lat.-vel. map for l = 169.5 deg, b < -10 deg vb_700p.fit Lat.-vel. map for l = 170.0 deg, b > +10 deg vb_700n.fit Lat.-vel. map for l = 170.0 deg, b < -10 deg vb_701n.fit Lat.-vel. map for l = 170.5 deg, b < -10 deg vb_701p.fit Lat.-vel. map for l = 170.5 deg, b > +10 deg vb_702p.fit Lat.-vel. map for l = 171.0 deg, b > +10 deg vb_702n.fit Lat.-vel. map for l = 171.0 deg, b < -10 deg vb_703n.fit Lat.-vel. map for l = 171.5 deg, b < -10 deg vb_703p.fit Lat.-vel. map for l = 171.5 deg, b > +10 deg vb_704n.fit Lat.-vel. map for l = 172.0 deg, b < -10 deg vb_704p.fit Lat.-vel. map for l = 172.0 deg, b > +10 deg vb_705n.fit Lat.-vel. map for l = 172.5 deg, b < -10 deg vb_705p.fit Lat.-vel. map for l = 172.5 deg, b > +10 deg vb_706p.fit Lat.-vel. map for l = 173.0 deg, b > +10 deg vb_706n.fit Lat.-vel. map for l = 173.0 deg, b < -10 deg vb_707p.fit Lat.-vel. map for l = 173.5 deg, b > +10 deg vb_707n.fit Lat.-vel. map for l = 173.5 deg, b < -10 deg vb_708p.fit Lat.-vel. map for l = 174.0 deg, b > +10 deg vb_708n.fit Lat.-vel. map for l = 174.0 deg, b < -10 deg vb_709p.fit Lat.-vel. map for l = 174.5 deg, b > +10 deg vb_709n.fit Lat.-vel. map for l = 174.5 deg, b < -10 deg vb_710p.fit Lat.-vel. map for l = 175.0 deg, b > +10 deg vb_710n.fit Lat.-vel. map for l = 175.0 deg, b < -10 deg vb_711p.fit Lat.-vel. map for l = 175.5 deg, b > +10 deg vb_711n.fit Lat.-vel. map for l = 175.5 deg, b < -10 deg vb_712p.fit Lat.-vel. map for l = 176.0 deg, b > +10 deg vb_712n.fit Lat.-vel. map for l = 176.0 deg, b < -10 deg vb_713n.fit Lat.-vel. map for l = 176.5 deg, b < -10 deg vb_713p.fit Lat.-vel. map for l = 176.5 deg, b > +10 deg vb_714p.fit Lat.-vel. map for l = 177.0 deg, b > +10 deg vb_714n.fit Lat.-vel. map for l = 177.0 deg, b < -10 deg vb_715p.fit Lat.-vel. map for l = 177.5 deg, b > +10 deg vb_715n.fit Lat.-vel. map for l = 177.5 deg, b < -10 deg vb_716p.fit Lat.-vel. map for l = 178.0 deg, b > +10 deg vb_716n.fit Lat.-vel. map for l = 178.0 deg, b < -10 deg vb_717n.fit Lat.-vel. map for l = 178.5 deg, b < -10 deg vb_717p.fit Lat.-vel. map for l = 178.5 deg, b > +10 deg vb_718n.fit Lat.-vel. map for l = 179.0 deg, b < -10 deg vb_718p.fit Lat.-vel. map for l = 179.0 deg, b > +10 deg vb_719p.fit Lat.-vel. map for l = 179.5 deg, b > +10 deg vb_719n.fit Lat.-vel. map for l = 179.5 deg, b < -10 deg Seth Digel C.-H. Joseph Lyu Hughes STX/NASA 1997 Mar 18 The General Information on High-latitude 21-cm Line Surveys by Carl Heiles (1988), University of California, Berkeley was used in creating this ReadMe file. UNKNOWN UNKNOWN In each catalog record, the corresponding VLSRs for the measured antenna temperatures can be obtained by the following FORTRAN statements. cvel = CenVel * 0.001 in units of km/s vwide = (30.e3/1420.4058e6)*2.998e5 vnarr = (10.e3/1420.4058e6)*2.998e5 if (cvel.eq.0.) then do i = 1,8 VLSR(i) = real(i-1)*vwide - 90.76 enddo do i = 9,95 VLSR(i) = real(i-9)*vnarr/2. - 45.38 enddo do i = 96,100 VLSR(i) = real(i-96)*vwide + 46.43 enddo else if (cvel.eq.-8.44) then do i = 1,8 VLSR(i) = real(i-1)*vwide - 82.32 enddo do i = 9,95 VLSR(i) = real(i-9)*vnarr/2. - 36.94 enddo do i = 96,100 VLSR(i) = real(i-96)*vwide + 54.87 enddo else print *,'unrecognized central velocity' endif end Brief description of software: FORTRAN codes for use in extracting spectra from the H I surveys of Heiles and Habing, Parkes, Argentina, Bell Labs, and Weaver and Williams. Most of the filters have a width of 10 kHz, corresponding to 2.11 km/s. They were overlapped by half of their width. The first 8 and last 5 filters are 30 kHz wide, corresponding to 6.33 km/s. There was no overlap in the frequency coverage of these filters. There is no previous ADC documentation for this catalog. VIII_7A.xml The Parkes High-Latitude H I Survey 8008A VIII/8A Parkes High-Latitude H I Survey The Parkes High-Latitude H I Survey M N Cleary C Heiles C G T Haslam Astron. & Astrophys. Suppl. 36 95 1979 1979A&AS...36...95C Radio sources Surveys H I data This survey consists of H I 21-cm spectra covering the southern sky with absolute galactic latitude |b| >= 10 degrees and declination <= -30 degrees. The observations were made with the Parkes Radio Observatory (CSIRO) 60-foot telescope. The receiver back end was the Parkes 64-channel spectrometer. The velocity resolution was 7 km/sec (33 kHz) and the beamwidth (HPBW) was 48 arcmin. Drift scans at constant declination were used with continuous integration in right ascension for -80 degrees <= declination <= -30 degrees. For declination < -80 degrees a grid of positions spaced 1 degree apart in declination and one beam-width apart in right ascension were observed. The survey was made in two parts. Part 1 included b >= -25 degrees, |b| >= 10 degrees and declination <= -30 degrees. Part 2 included b <= -25 degrees and declination <= -30 degrees. The scans in Part 1 were spaced at 1 degree intervals in declination and the velocity coverage was from -148 to +300 km/sec. The scans in Part 2 were spaced at 2 degrees and the velocity coverage was from -230 to +218 km/sec. Each spectrum or record consists of a header followed by 64 antenna temperatures. The header contains the galactic longitude, galactic latitude, right ascension, declination, central velocity (LSR), and quality factor. The catalog contains a total of 9891 spectra.
lbmap.fit Velocity-integrated map of the whole plane vb_098.fit Latitude-velocity map for l = -131.0 deg vb_099.fit Latitude-velocity map for l = -130.5 deg vb_100.fit Latitude-velocity map for l = -130.0 deg vb_101.fit Latitude-velocity map for l = -129.5 deg vb_102.fit Latitude-velocity map for l = -129.0 deg vb_103.fit Latitude-velocity map for l = -128.5 deg vb_104.fit Latitude-velocity map for l = -128.0 deg vb_105.fit Latitude-velocity map for l = -127.5 deg vb_106.fit Latitude-velocity map for l = -127.0 deg vb_107.fit Latitude-velocity map for l = -126.5 deg vb_108.fit Latitude-velocity map for l = -126.0 deg vb_109.fit Latitude-velocity map for l = -125.5 deg vb_110.fit Latitude-velocity map for l = -125.0 deg vb_111.fit Latitude-velocity map for l = -124.5 deg vb_112.fit Latitude-velocity map for l = -124.0 deg vb_113.fit Latitude-velocity map for l = -123.5 deg vb_114.fit Latitude-velocity map for l = -123.0 deg vb_115.fit Latitude-velocity map for l = -122.5 deg vb_116.fit Latitude-velocity map for l = -122.0 deg vb_117.fit Latitude-velocity map for l = -121.5 deg vb_118.fit Latitude-velocity map for l = -121.0 deg vb_119.fit Latitude-velocity map for l = -120.5 deg vb_120.fit Latitude-velocity map for l = -120.0 deg vb_121.fit Latitude-velocity map for l = -119.5 deg vb_122.fit Latitude-velocity map for l = -119.0 deg vb_123.fit Latitude-velocity map for l = -118.5 deg vb_124.fit Latitude-velocity map for l = -118.0 deg vb_125.fit Latitude-velocity map for l = -117.5 deg vb_126.fit Latitude-velocity map for l = -117.0 deg vb_127.fit Latitude-velocity map for l = -116.5 deg vb_128.fit Latitude-velocity map for l = -116.0 deg vb_129.fit Latitude-velocity map for l = -115.5 deg vb_130.fit Latitude-velocity map for l = -115.0 deg vb_131.fit Latitude-velocity map for l = -114.5 deg vb_132.fit Latitude-velocity map for l = -114.0 deg vb_133.fit Latitude-velocity map for l = -113.5 deg vb_134.fit Latitude-velocity map for l = -113.0 deg vb_135.fit Latitude-velocity map for l = -112.5 deg vb_136.fit Latitude-velocity map for l = -112.0 deg vb_137.fit Latitude-velocity map for l = -111.5 deg vb_138.fit Latitude-velocity map for l = -111.0 deg vb_139.fit Latitude-velocity map for l = -110.5 deg vb_140.fit Latitude-velocity map for l = -110.0 deg vb_141.fit Latitude-velocity map for l = -109.5 deg vb_142.fit Latitude-velocity map for l = -109.0 deg vb_143.fit Latitude-velocity map for l = -108.5 deg vb_144.fit Latitude-velocity map for l = -108.0 deg vb_145.fit Latitude-velocity map for l = -107.5 deg vb_146.fit Latitude-velocity map for l = -107.0 deg vb_147.fit Latitude-velocity map for l = -106.5 deg vb_148.fit Latitude-velocity map for l = -106.0 deg vb_149.fit Latitude-velocity map for l = -105.5 deg vb_150.fit Latitude-velocity map for l = -105.0 deg vb_151.fit Latitude-velocity map for l = -104.5 deg vb_152.fit Latitude-velocity map for l = -104.0 deg vb_153.fit Latitude-velocity map for l = -103.5 deg vb_154.fit Latitude-velocity map for l = -103.0 deg vb_155.fit Latitude-velocity map for l = -102.5 deg vb_156.fit Latitude-velocity map for l = -102.0 deg vb_157.fit Latitude-velocity map for l = -101.5 deg vb_158.fit Latitude-velocity map for l = -101.0 deg vb_159.fit Latitude-velocity map for l = -100.5 deg vb_160.fit Latitude-velocity map for l = -100.0 deg vb_161.fit Latitude-velocity map for l = -99.5 deg vb_162.fit Latitude-velocity map for l = -99.0 deg vb_163.fit Latitude-velocity map for l = -98.5 deg vb_164.fit Latitude-velocity map for l = -98.0 deg vb_165.fit Latitude-velocity map for l = -97.5 deg vb_166.fit Latitude-velocity map for l = -97.0 deg vb_167.fit Latitude-velocity map for l = -96.5 deg vb_168.fit Latitude-velocity map for l = -96.0 deg vb_169.fit Latitude-velocity map for l = -95.5 deg vb_170.fit Latitude-velocity map for l = -95.0 deg vb_171.fit Latitude-velocity map for l = -94.5 deg vb_172.fit Latitude-velocity map for l = -94.0 deg vb_173.fit Latitude-velocity map for l = -93.5 deg vb_174.fit Latitude-velocity map for l = -93.0 deg vb_175.fit Latitude-velocity map for l = -92.5 deg vb_176.fit Latitude-velocity map for l = -92.0 deg vb_177.fit Latitude-velocity map for l = -91.5 deg vb_178.fit Latitude-velocity map for l = -91.0 deg vb_179.fit Latitude-velocity map for l = -90.5 deg vb_180.fit Latitude-velocity map for l = -90.0 deg vb_181.fit Latitude-velocity map for l = -89.5 deg vb_182.fit Latitude-velocity map for l = -89.0 deg vb_183.fit Latitude-velocity map for l = -88.5 deg vb_184.fit Latitude-velocity map for l = -88.0 deg vb_185.fit Latitude-velocity map for l = -87.5 deg vb_186.fit Latitude-velocity map for l = -87.0 deg vb_187.fit Latitude-velocity map for l = -86.5 deg vb_188.fit Latitude-velocity map for l = -86.0 deg vb_189.fit Latitude-velocity map for l = -85.5 deg vb_190.fit Latitude-velocity map for l = -85.0 deg vb_191.fit Latitude-velocity map for l = -84.5 deg vb_192.fit Latitude-velocity map for l = -84.0 deg vb_193.fit Latitude-velocity map for l = -83.5 deg vb_194.fit Latitude-velocity map for l = -83.0 deg vb_195.fit Latitude-velocity map for l = -82.5 deg vb_196.fit Latitude-velocity map for l = -82.0 deg vb_197.fit Latitude-velocity map for l = -81.5 deg vb_198.fit Latitude-velocity map for l = -81.0 deg vb_199.fit Latitude-velocity map for l = -80.5 deg vb_200.fit Latitude-velocity map for l = -80.0 deg vb_201.fit Latitude-velocity map for l = -79.5 deg vb_202.fit Latitude-velocity map for l = -79.0 deg vb_203.fit Latitude-velocity map for l = -78.5 deg vb_204.fit Latitude-velocity map for l = -78.0 deg vb_205.fit Latitude-velocity map for l = -77.5 deg vb_206.fit Latitude-velocity map for l = -77.0 deg vb_207.fit Latitude-velocity map for l = -76.5 deg vb_208.fit Latitude-velocity map for l = -76.0 deg vb_209.fit Latitude-velocity map for l = -75.5 deg vb_210.fit Latitude-velocity map for l = -75.0 deg vb_211.fit Latitude-velocity map for l = -74.5 deg vb_212.fit Latitude-velocity map for l = -74.0 deg vb_213.fit Latitude-velocity map for l = -73.5 deg vb_214.fit Latitude-velocity map for l = -73.0 deg vb_215.fit Latitude-velocity map for l = -72.5 deg vb_216.fit Latitude-velocity map for l = -72.0 deg vb_217.fit Latitude-velocity map for l = -71.5 deg vb_218.fit Latitude-velocity map for l = -71.0 deg vb_219.fit Latitude-velocity map for l = -70.5 deg vb_220.fit Latitude-velocity map for l = -70.0 deg vb_221.fit Latitude-velocity map for l = -69.5 deg vb_222.fit Latitude-velocity map for l = -69.0 deg vb_223.fit Latitude-velocity map for l = -68.5 deg vb_224.fit Latitude-velocity map for l = -68.0 deg vb_225.fit Latitude-velocity map for l = -67.5 deg vb_226.fit Latitude-velocity map for l = -67.0 deg vb_227.fit Latitude-velocity map for l = -66.5 deg vb_228.fit Latitude-velocity map for l = -66.0 deg vb_229.fit Latitude-velocity map for l = -65.5 deg vb_230.fit Latitude-velocity map for l = -65.0 deg vb_231.fit Latitude-velocity map for l = -64.5 deg vb_232.fit Latitude-velocity map for l = -64.0 deg vb_233.fit Latitude-velocity map for l = -63.5 deg vb_234.fit Latitude-velocity map for l = -63.0 deg vb_235.fit Latitude-velocity map for l = -62.5 deg vb_236.fit Latitude-velocity map for l = -62.0 deg vb_237.fit Latitude-velocity map for l = -61.5 deg vb_238.fit Latitude-velocity map for l = -61.0 deg vb_239.fit Latitude-velocity map for l = -60.5 deg vb_240.fit Latitude-velocity map for l = -60.0 deg vb_241.fit Latitude-velocity map for l = -59.5 deg vb_242.fit Latitude-velocity map for l = -59.0 deg vb_243.fit Latitude-velocity map for l = -58.5 deg vb_244.fit Latitude-velocity map for l = -58.0 deg vb_245.fit Latitude-velocity map for l = -57.5 deg vb_246.fit Latitude-velocity map for l = -57.0 deg vb_247.fit Latitude-velocity map for l = -56.5 deg vb_248.fit Latitude-velocity map for l = -56.0 deg vb_249.fit Latitude-velocity map for l = -55.5 deg vb_250.fit Latitude-velocity map for l = -55.0 deg vb_251.fit Latitude-velocity map for l = -54.5 deg vb_252.fit Latitude-velocity map for l = -54.0 deg vb_253.fit Latitude-velocity map for l = -53.5 deg vb_254.fit Latitude-velocity map for l = -53.0 deg vb_255.fit Latitude-velocity map for l = -52.5 deg vb_256.fit Latitude-velocity map for l = -52.0 deg vb_257.fit Latitude-velocity map for l = -51.5 deg vb_258.fit Latitude-velocity map for l = -51.0 deg vb_259.fit Latitude-velocity map for l = -50.5 deg vb_260.fit Latitude-velocity map for l = -50.0 deg vb_261.fit Latitude-velocity map for l = -49.5 deg vb_262.fit Latitude-velocity map for l = -49.0 deg vb_263.fit Latitude-velocity map for l = -48.5 deg vb_264.fit Latitude-velocity map for l = -48.0 deg vb_265.fit Latitude-velocity map for l = -47.5 deg vb_266.fit Latitude-velocity map for l = -47.0 deg vb_267.fit Latitude-velocity map for l = -46.5 deg vb_268.fit Latitude-velocity map for l = -46.0 deg vb_269.fit Latitude-velocity map for l = -45.5 deg vb_270.fit Latitude-velocity map for l = -45.0 deg vb_271.fit Latitude-velocity map for l = -44.5 deg vb_272.fit Latitude-velocity map for l = -44.0 deg vb_273.fit Latitude-velocity map for l = -43.5 deg vb_274.fit Latitude-velocity map for l = -43.0 deg vb_275.fit Latitude-velocity map for l = -42.5 deg vb_276.fit Latitude-velocity map for l = -42.0 deg vb_277.fit Latitude-velocity map for l = -41.5 deg vb_278.fit Latitude-velocity map for l = -41.0 deg vb_279.fit Latitude-velocity map for l = -40.5 deg vb_280.fit Latitude-velocity map for l = -40.0 deg vb_281.fit Latitude-velocity map for l = -39.5 deg vb_282.fit Latitude-velocity map for l = -39.0 deg vb_283.fit Latitude-velocity map for l = -38.5 deg vb_284.fit Latitude-velocity map for l = -38.0 deg vb_285.fit Latitude-velocity map for l = -37.5 deg vb_286.fit Latitude-velocity map for l = -37.0 deg vb_287.fit Latitude-velocity map for l = -36.5 deg vb_288.fit Latitude-velocity map for l = -36.0 deg vb_289.fit Latitude-velocity map for l = -35.5 deg vb_290.fit Latitude-velocity map for l = -35.0 deg vb_291.fit Latitude-velocity map for l = -34.5 deg vb_292.fit Latitude-velocity map for l = -34.0 deg vb_293.fit Latitude-velocity map for l = -33.5 deg vb_294.fit Latitude-velocity map for l = -33.0 deg vb_295.fit Latitude-velocity map for l = -32.5 deg vb_296.fit Latitude-velocity map for l = -32.0 deg vb_297.fit Latitude-velocity map for l = -31.5 deg vb_298.fit Latitude-velocity map for l = -31.0 deg vb_299.fit Latitude-velocity map for l = -30.5 deg vb_300.fit Latitude-velocity map for l = -30.0 deg vb_301.fit Latitude-velocity map for l = -29.5 deg vb_302.fit Latitude-velocity map for l = -29.0 deg vb_303.fit Latitude-velocity map for l = -28.5 deg vb_304.fit Latitude-velocity map for l = -28.0 deg vb_305.fit Latitude-velocity map for l = -27.5 deg vb_306.fit Latitude-velocity map for l = -27.0 deg vb_307.fit Latitude-velocity map for l = -26.5 deg vb_308.fit Latitude-velocity map for l = -26.0 deg vb_309.fit Latitude-velocity map for l = -25.5 deg vb_310.fit Latitude-velocity map for l = -25.0 deg vb_311.fit Latitude-velocity map for l = -24.5 deg vb_312.fit Latitude-velocity map for l = -24.0 deg vb_313.fit Latitude-velocity map for l = -23.5 deg vb_314.fit Latitude-velocity map for l = -23.0 deg vb_315.fit Latitude-velocity map for l = -22.5 deg vb_316.fit Latitude-velocity map for l = -22.0 deg vb_317.fit Latitude-velocity map for l = -21.5 deg vb_318.fit Latitude-velocity map for l = -21.0 deg vb_319.fit Latitude-velocity map for l = -20.5 deg vb_320.fit Latitude-velocity map for l = -20.0 deg vb_321.fit Latitude-velocity map for l = -19.5 deg vb_322.fit Latitude-velocity map for l = -19.0 deg vb_323.fit Latitude-velocity map for l = -18.5 deg vb_324.fit Latitude-velocity map for l = -18.0 deg vb_325.fit Latitude-velocity map for l = -17.5 deg vb_326.fit Latitude-velocity map for l = -17.0 deg vb_327.fit Latitude-velocity map for l = -16.5 deg vb_328.fit Latitude-velocity map for l = -16.0 deg vb_329.fit Latitude-velocity map for l = -15.5 deg vb_330.fit Latitude-velocity map for l = -15.0 deg vb_331.fit Latitude-velocity map for l = -14.5 deg vb_332.fit Latitude-velocity map for l = -14.0 deg vb_333.fit Latitude-velocity map for l = -13.5 deg vb_334.fit Latitude-velocity map for l = -13.0 deg vb_335.fit Latitude-velocity map for l = -12.5 deg vb_336.fit Latitude-velocity map for l = -12.0 deg vb_337.fit Latitude-velocity map for l = -11.5 deg vb_338.fit Latitude-velocity map for l = -11.0 deg vb_339.fit Latitude-velocity map for l = -10.5 deg vb_340.fit Latitude-velocity map for l = -10.0 deg vb_341.fit Latitude-velocity map for l = -9.5 deg vb_342.fit Latitude-velocity map for l = -9.0 deg vb_343.fit Latitude-velocity map for l = -8.5 deg vb_344.fit Latitude-velocity map for l = -8.0 deg vb_345.fit Latitude-velocity map for l = -7.5 deg vb_346.fit Latitude-velocity map for l = -7.0 deg vb_347.fit Latitude-velocity map for l = -6.5 deg vb_348.fit Latitude-velocity map for l = -6.0 deg vb_349.fit Latitude-velocity map for l = -5.5 deg vb_350.fit Latitude-velocity map for l = -5.0 deg vb_351.fit Latitude-velocity map for l = -4.5 deg vb_352.fit Latitude-velocity map for l = -4.0 deg vb_353.fit Latitude-velocity map for l = -3.5 deg vb_354.fit Latitude-velocity map for l = -3.0 deg vb_355.fit Latitude-velocity map for l = -2.5 deg vb_356.fit Latitude-velocity map for l = -2.0 deg vb_357.fit Latitude-velocity map for l = -1.5 deg vb_358.fit Latitude-velocity map for l = -1.0 deg vb_359.fit Latitude-velocity map for l = -0.5 deg vb_360.fit Latitude-velocity map for l = 0.0 deg vb_361.fit Latitude-velocity map for l = 0.5 deg vb_362.fit Latitude-velocity map for l = 1.0 deg vb_363.fit Latitude-velocity map for l = 1.5 deg vb_364.fit Latitude-velocity map for l = 2.0 deg vb_365.fit Latitude-velocity map for l = 2.5 deg vb_366.fit Latitude-velocity map for l = 3.0 deg vb_367.fit Latitude-velocity map for l = 3.5 deg vb_368.fit Latitude-velocity map for l = 4.0 deg vb_369.fit Latitude-velocity map for l = 4.5 deg vb_370.fit Latitude-velocity map for l = 5.0 deg vb_371.fit Latitude-velocity map for l = 5.5 deg vb_372.fit Latitude-velocity map for l = 6.0 deg vb_373.fit Latitude-velocity map for l = 6.5 deg vb_374.fit Latitude-velocity map for l = 7.0 deg vb_375.fit Latitude-velocity map for l = 7.5 deg vb_376.fit Latitude-velocity map for l = 8.0 deg vb_377.fit Latitude-velocity map for l = 8.5 deg vb_378.fit Latitude-velocity map for l = 9.0 deg vb_379.fit Latitude-velocity map for l = 9.5 deg vb_380.fit Latitude-velocity map for l = 10.0 deg vb_381.fit Latitude-velocity map for l = 10.5 deg vb_382.fit Latitude-velocity map for l = 11.0 deg vb_383.fit Latitude-velocity map for l = 11.5 deg vb_384.fit Latitude-velocity map for l = 12.0 deg vb_385.fit Latitude-velocity map for l = 12.5 deg vb_386.fit Latitude-velocity map for l = 13.0 deg vb_387.fit Latitude-velocity map for l = 13.5 deg vb_388.fit Latitude-velocity map for l = 14.0 deg vb_389.fit Latitude-velocity map for l = 14.5 deg vb_390.fit Latitude-velocity map for l = 15.0 deg Seth Digel C.-H. Joseph Lyu Hughes STX/NASA 1997 Mar 24 The General Information on High-latitude 21-cm Line Surveys by Carl Heiles (1988), University of California, Berkeley was used to create this ReadMe file. UNKNOWN UNKNOWN A FITS version of the survey was derived at the Astrophysics Data Facility (NASA/GSFC) from the original catalog of spectra. Of the 9891 spectra in the catalog, 59 were rejected for having spikes, ridges, or bad baselines. (The 'quality' flag in the original catalog is undocumented and its value does not seem to be correlated with the appearance of the spectra; it was ignored.) The remaining 9832 spectra were interpolated in frequency to a uniform central velocity, then interpolated spatially onto a regular grid in Galactic coordinates. For the latter interpolation, the cos(b) corrections for longitude offsets were taken into account. Owing to the sparse sampling, especially at high latitudes, interpolation over several degrees was frequently required. The effective angular resolution of the FITS maps varies from about 1 degree to at least 3 degrees. Latitude-velocity slices were written in FITS format for each 30 arcmin of longitude. Longitude ranges containing no spectra were not written. A longitude- latitude map, integrated over all velocities, was also written in FITS format to illustrate the coverage of the individual latitude-velocity slices. Note that in many spectra the emission extends beyond the velocity coverage of the spectrometer. High-velocity emission, in particular parts of the Magellanic Stream, may have been missed in the observations; see Mathewson et al. (1974 and 1977). VIII_8A.xml The Argentina High-Latitude H I Survey 8009 VIII/9 Argentina High-Latitude H I Survey The Argentina High-Latitude H I Survey F R Colomb W G L Poppel C Heiles Astron. & Astrophys. Suppl. 40 47 1980 1980A&AS...40...47C Radio sources Surveys H I data This survey consists of H I 21-cm spectra covering the southern sky with absolute galactic latitude |b| >10 degrees and a declination <-25 degrees. The observations were made with the 30 m telescope of the Instituto Argentino de Radioastronomia during 1973 to 1977 and were described in (Colomb et al. 1977). The data were obtained by keeping the telescope fixed on the meridian at the desired declination and letting the sky drift through the field. The individual spectra were obtained with a 56-channel filterbank and covering the velocity range from about -40 to +40 km/sec. The velocity resolution is 2 km/sec, and the beamwidth is 30 arcmin. Each spectrum or record consists of a header followed by 56 antenna temperatures. The header contains the galactic longitude, galactic latitude, right ascension (1950), declination (1950), date (local standard time), date of observation (year, month, day), bad scan information, velocity (LSR) of channel 1, velocity (LSR) of channel 56, and a quality factor. The catalog contains a total of 55470 spectra.
Southern sky survey data GLONm Galactic longitude in units of 0.001 degrees 0.001deg GLATm Galactic latitude in units of 0.001 degrees 0.001deg RAh Right ascension (1950) h RAm RA in minutes (1950) min RAs RA in seconds (1950) s DE- Sign of declination --- DEd DEC in degree (1950) deg DEm DEC in arcminutes (1950) arcmin DEs DEC in arcseconds (1950) arcsec LSTh Local Standard Time (LST) in hours h LSTm LST in minutes min LSTs LST in seconds s ObsDate Date of observation in yymmdd (year month day) --- Bscan1 Bad scan number 1 --- Bscan2 Bad scan number 2 --- Bscan3 Bad scan number 3 --- Bscan4 Bad scan number 4 --- Bscan5 Bad scan number 5 --- CenVel1 Central velocity at channel 1 0.01km/s CenVel56 Central velocity at channel 56 0.01km/s Qfactor Quality factor, 0 (set to zero) --- AntTemp Antenna temperature in units of 0.01K 0.01K C.-H. Joseph Lyu Hughes STX/NASA 1995 Dec 12 The General Information on High-latitude 21-cm Line Surveys by Carl Heiles (1988), University of California, Berkeley was used to create this ReadMe file. UNKNOWN UNKNOWN In each record, the corresponding VLSRs for the measured antenna temperatures can be obtained by the following statements. V1 = CenVel1 * 0.01 in units of km/s V56= CenVel56* 0.01 dv = (V56-V1)/55. Do i = 1, 56 VLSR(i)= V1 + (i-1)* dv enddo Brief description of software: The included software contains FORTRAN codes for use in extracting spectra from the H I surveys of Heiles and Habing, Parkes, Argentina, Bell Labs, and Weaver and Williams. The data consist of 56-channel profiles sorted in Galactic latitude and longitude. The data were obtained by holding the telescope fixed and letting the sky drift through. Thus the natural coordinate system for the data is in celestial coordinates, so the data are not gridded in Galactic coordinates. This survey has good velocity and angular resolution, so is good for examining the structure of narrow features. There was no previous ADC documentation for this catalog. VIII_9.xml The Berkeley Low-Latitude Survey of Neutral Hydrogen 8011 VIII/11 Berkeley Low-Latitude H I Survey The Berkeley Low-Latitude Survey of Neutral Hydrogen H Weaver D R W Williams Astron. & Astrophys. Suppl. 8 1 1973 1973A&AS....8....1W Radio sources Surveys H I data This survey consists of H I 21-cm spectra covering galactic latitudes from -10 degrees to +10 degrees and galactic longitudes from 10 degrees to 250 degrees. The observations were made with the Hat Creek 85-foot telescope between 1968 and 1970. The individual spectra contain 238 points per profile and cover a velocity range of 250 km/s. The velocity resolution is 2 km/sec (half-power of each filter) and the half-power beamwidth is 35 arcmin. The spacing between points observed on the sky are 0.25 degrees in galactic latitude and 0.5 degrees in galactic longitude. Each spectrum or record consists of a header followed by 238 antenna temperatures. The header contains the galactic longitude, galactic latitude, and central velocity (lsr). The catalog contains a total of 38961 spectra.
Low latitude H I Survey Data GLONm Galactic Longitude 0.1deg GLATm Galactic Latitude 0.01deg CenVel Central Velocity (Local Standard of Rest) 0.1km/s AntTemp Antenna temperature 0.1K C.-H. Joseph Lyu Hughes STX/NASA 1995 Dec 12 UNKNOWN UNKNOWN In each record, the corresponding VLSRs for the measured antenna temperatures can be obtained by the following statements. cvel = CenVel * 0.1 in units of km/s Do i = 1, 238 VLSR(i)= cvel + (i-122.)* 1.0553 enddo Brief description of software: The included software contains FORTRAN code for use in extracting spectra from the H I surveys of Heiles and Habing, Parkes, Argentina, Bell Labs, and Weaver and Williams. There was no previous ADC documentation for this catalog. The data format described in the "software" was used to create Byte-by-byte Description of this ReadMe file. VIII_11.xml Orion A Emission-Line Surveys from 200.7-202.3, 203.7-205.3, and 330.5-360.1 GHz 8012 VIII/12 Orion A Emission-Line Surveys Orion A Emission-Line Surveys from 200.7-202.3, 203.7-205.3, and 330.5-360.1 GHz P R Jewell J M Hollis F J Lovas L E Snyder Astrophys. Journ. Suppl. 70 833 1989 1989ApJS...70..833J Radio sources Surveys This catalog comprised surveys of the Orion A molecular emission lines from 200.7-202.3, 203.7-205.3, and 330.5-360.1 GHz. These surveys were done by using the 12 m radio telescope of the National Radio Astronomy Observatory (NRAO). For the 870 microns (um) atmospheric window, about 160 distinct spectral features composed of nearly 180 lines were detected. For the other two bands 42 distinct, new spectral lines were detected. The new interstellar lines in the survey bands were tabulated in FITS format. This new data base would be a useful resource for further analyses of abundances and excitation of known Orion A species and for determining unidentified lines for use in molecule identification. The single-dish FITS format in FITS table extension was adopted to create this catalog. The data were tabulated in the order of Figures 1-39, including both the unshifted and shifted spectra in each figure (Jewell et al., 1989). Single Dish header parameters were represented in the table's header, and the data comprised the actual table in ASCII. Various FITS Tables keywords were given in great detail for describing the format of the table and how a computer program could read it.
figs.fit Orion A Survey data in FITS format C.-H. Joseph Lyu Hughes STX/NASA 1996 May 22 The original journal paper (Jewell et al. 1989), CDS Intro file, and the memo of the Single Dish FITS tape by Betty Stobie and Lorrie Morgan (1986) were used to create this ReadMe file. UNKNOWN UNKNOWN The Orion A survey data were received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Phil Jewell on September 10, 1990. The data images of the spectra were written in the exact order that the figures appear in the journal paper. The lower sideband (LSB) frequencies (in MHz) of the 75 tables were summarized in the following list (table number vs. LSB): No. LSB(MHz) No. LSB(MHz) No. LSB(MHz) 1 201003 26 339810 51 351810 2 201515 27 339800 52 353300 3 202027 28 343300 53 353310 4 333800 29 343310 54 353800 5 333810 30 343800 55 353880 6 334300 31 343810 56 354300 7 334310 32 344300 57 354310 8 334800 33 344310 58 355300 9 334810 34 344800 59 355310 10 335300 35 344810 60 355800 11 335310 36 345300 61 355810 12 335800 37 345310 62 356300 13 335810 38 345796 63 356310 14 336300 39 345806 64 357300 15 336310 40 349300 65 357290 16 337300 41 349310 66 357800 17 337310 42 349800 67 357810 18 337800 43 349810 68 358300 19 337810 44 350300 69 358310 20 338300 45 350310 70 358800 21 338310 46 350800 71 358810 22 338800 47 350810 72 359300 23 338810 48 351300 73 359310 24 339300 49 351310 74 359800 25 339310 50 351800 75 359810 Note the 75 FITS tables correspond to the Figures 1-39 of Jewell et al. (1989). VIII_12.xml A new catalog of 53522 4.85GHz sources 8013 VIII/13 A new catalog of 53522 4.85GHz sources A new catalog of 53522 4.85GHz sources R H Becker R L White A L Edwards Astrohys. J., Suppl. Ser. 75 1-229 1991 1991ApJS...75....1B Radio sources A catalog of 53522 4.85GHz sources between 0 and 75 degrees declination has been generated from observations taken with the NRAO Green Blank 300foot (91m) telescope. The flux limit of the catalog is dependent on declination and ranges from about 40mJy at 0degree to 20mJy at 60degrees. The source positions given in the catalog have a 95% confidence radius of about 50arcsec. Spectral indices have been calculated for 29051 sources which have counterparts in the Texas 365MHz northern sky survey.
The catalogue of radio sources Name 6-cm Name, constructed from position HHMM+DDSS, with A or B added at end if needed to make name unique --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec Flux at 4.85-GHz (mJy) mJy extFlag "*" if source is extended, else blank --- SpIndex Spectral index between 4.85GHz and 0.365GHz number=1 The spectral index {alpha} is d(log(Flux))/d(log(Frequency)) i.e. F{nu} {proportional.to} {nu}^{alpha}^ The 365GHz flux is from Texas survey, Douglas et al., private comm. --- n_SpIndex "*" if separation between 4.85GHz and 0.365GHz positions is greater than 100 arcsec, else blank --- Francois Ochsenbein CDS 1995 May 02 UNKNOWN UNKNOWN * 21-Jul-1992: Received from ADC * 02-May-1995: documentation standardized UNKNOWN UNKNOWN FORTRAN reading: The following Fortran statements can be used to read the file: character name*10, decsgn*1, extflg, widflg integer rah, ram, decd, decm, decs, flux real rass, spind read(10,1) name, rah, ram, ras, decsgn, decd, decm, decs, & flux, extflg, spind, widflg 1 format(a10,1x,i2, 1x, i2, 1x, f4.1, 1x, a1, i2, 1x, i2, 1x, i2, & i6, a1, 1x, f4.1, a1) VIII_13.xml The 87GB Catalog of Radio Sources Covering 0d < Dec <+75d at 4.85 GHz 8014 VIII/14 87GB Radio Sources 4.85 GHz The 87GB Catalog of Radio Sources Covering 0d < Dec <+75d at 4.85 GHz P C Gregory J J Condon Astrophys. J. Suppl. Ser. 75 1011-1291 1991 1991ApJS...75.1011G Radio sources The Green Bank 300-foot (91 m) telescope was used during 1987 October to map 6.0 sr of sky in the 0 deg to +75 deg declination band at 4.85 GHz. The 87GB catalog of 54579 discrete sources with angular sizes <10.5 arcmin and flux densities larger than S ~25-40 mJy was derived from these maps The catalog positions and flux densities have been corrected for known map biases. Their estimated uncertainties were verified by comparisons with more accurate positions and flux densities available for some sources. The file names specify the equinox and hour of right ascension; e.g., B1950.00H or J2000.23H. The data also give the sources' galactic latitudes and longitudes, fitted major axes, minor axes, and position angles, the local sky levels (baseline zero offsets of the Gaussian fits), and map pixel coordinates.
readme.txt Introduction from Green Bank CD-ROM b1950.fit The 87GB Catalogue in B1950 coordinates j2000.fit The 87GB Catalogue in J2000 coordinates Francois Ochsenbein CDS C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 02 The original CDS documentation by Francois Ochsenbein (1992) and "Introduction of Green Bank CD-ROM" by J. J. Condon were used to create this ReadMe file. UNKNOWN UNKNOWN The 54579 sources of the 87GB catalogue are stored as FITS files (ascii table FITS), with B1950 coordinates (b1950.fit) and J2000 coordinates (j2000.fit). On Unix workstations, a simple fold command can be used to transform the FITS files into plain ascii files with the following format: Bytes Format Units Label Explanations 1- 2 I2 hr RAh right ascension (hours) [B1950 or J2000] 3- 4 I2 min RAm right ascension (minutes) 5- 8 F4.1 s RAs right ascension (seconds) 10- 12 F3.1 s u_RAs rms uncertainty in RAs (seconds) 14- 14 A1 DE- declination sign 15- 16 I2 deg DEd declination (degrees) [B1950 or J2000] 17- 18 I2 arcmin DEm declination (minutes) 19- 20 I2 arcsec DEs declination (seconds) 22- 23 I2 arcsec u_DEs rms uncertainty in DEs 25- 29 F5.1 deg GLAT galactic latitude b(II) 31- 35 F5.1 deg GLON galactic longitude l(II) 37- 41 I5 mJy FLUX 4.85 GHz peak flux density 43- 46 I5 mJy u_FLUX rms uncertainty in FLUX 49- 49 A1 EFLAG flag for extended source 50- 50 A1 WFLAG warning flag 51- 51 A1 CFLAG flag for confused source 53- 56 F4.2 PHIMAJ normalized major axis of fit 58- 61 F4.2 PHIMIN normalized minor axis of fit 63- 65 I3 deg ANGLE fit major-axis PA (degrees E of N) 67- 69 I5 mJy ZERO zero-level of fit 71- 74 I4 PIXX x-coordinate pixel number 76- 79 I4 PIXY y-coordinate pixel number Issuing on Unix workstations the command "make" in this directory should normally be enough to generate the search programs and their related data files (these programs do not use the FITS files, but plain ascii files B1950.xxH and J2000.xxH with the above format, where xx stands for the hour of right ascension from 00 to 23). VIII_14.xml Parkes Radio Sources Catalogue, Version 1.01 8015 VIII/15 Parkes Radio Sources Catalogue Parkes Radio Sources Catalogue, Version 1.01 A E Wright R Otrupcek Australia Telescope National Facility, Parkes ??? ??? 1990 1990 Radio sources PKSCAT90 consists of radio and optical data for 8264 radio sources. It covers essentially all the sky south of declination +27 degrees but largely excludes the Galactic Plane and the Magellanic Cloud regions. The latter zones have been the subject of other, specialist surveys. A few data errors in Version 1.00 have been corrected in the present edition. This version of the Parkes Radio source Catalogue entitled "PKSCAT90 Version 1.01" is intended for use on IBM PC-type machines. Note by A. Wright: Users should note that PKSCAT90 was produced at a time when relational databases were in their infancy. In the future we anticipate making the individual data sources available separately --- through such search systems as SIMBAD --- rather than in an "omnibus" catalogue like PKSCAT90. For both the Northern and Southern hemisphere, superior and deeper finding surveys now exist: the 87GB Catalog in the North, (Condon et al., catalog <VIII/14>) and the PMN catalogues (Griffith and Wright, catalog <VIII/38>) in the South.
The Catalogue Bname B1950 source name --- Alias Alias/other catalogue names --- RAh Right Ascension B1950.0 (hours) h RAm Right Ascension B1950.0 (minutes) min RAs Right Ascension B1950.0 (seconds) s DE- Declination B1950.0 (sign) --- DEd Declination B1950.0 (degrees) deg DEm Declination B1950.0 (minutes) arcmin DEs Declination B1950.0 (seconds) arcsec Ident Identification number=1 Beginning with this version of the catalogue, new identification and field classification codes have been used, mainly for the unidentified or "blank-field" sources. The following table lists both the new and the old codes. ------------------------------------------------------------------- Code Description Old Code ------------------------------------------------------------------- ===> Identified sources: BLC BL Lacertae object BLC D Diffuse galaxy, bright galaxies in clusters D DB Double galaxy DB E Elliptical Galaxy E G Galaxy too faint to classify G HII HII region HII IRR Irregular object IRR N N galaxy, bright cored galaxy N PN Planetary Nebular PN Q Quasi-stellar object or Quasar (confirmed) Q QC Quasar with a continuous optical spectrum QC S Spiral galaxy S SB Barred Spiral galaxy SB Sc Spiral galaxy (type C) SC SNR SuperNova Remnant SNR S0 Spiral galaxy with ellipticity of zero S0 (nearly circular) * Stellar object of neutral colour IIIS in good positional agreement with the radio source ===> Unidentified Sources Xg one or more galaxies in the area II covered by the position error of the source but no identification claimed Xs blank field: one or more stars of normal colour III in the error box Xsa blank field: obscured by absorption IIIA X blank field: no absorption apparent IIIB Xs+ blank field: crowded star field IIIC Xa blank field: heavily obscured. IV ------------------------------------------------------------------- NOTE: a ? following any code specifies that that property is uncertain ------------------------------------------------------------------- --- Mag Magnitude (the format is either F4.1 or F4.2) mag z Redshift (reference in r_z) --- S80 Flux density at 80 MHz Jy S178 Flux density at 178 MHz Jy S408 Flux density at 408 MHz Jy S635 Flux density at 635 MHz Jy S1410 Flux density at 1410 MHz (21cm) Jy S2700 Flux density at 2700 MHz (11cm) Jy S5000 Flux density at 5000 MHz (6cm) Jy S8400 Flux density at 8400 MHz Jy S22000 Flux density at 22000 MHz Jy RA2000h Right Ascension J2000 (hours) h RA2000m Right Ascension J2000 (minutes) min RA2000s Right Ascension J2000 (seconds) s DE2000- Declination J2000 (sign) --- DE2000d Declination J2000 (degrees) deg DE2000m Declination J2000 (minutes) arcmin DE2000s Declination J2000 (seconds) arcsec Jname J2000 Name --- errPos positional accuracy in arcsec. (to be read as "better than") arcsec r_Ident Comma-separated references for Identification (see file refs.dat) --- r_z Comma-separated references for z (see file refs.dat) --- SpDate Year.Month for which an optical spectrum was obtained, but from which a definite redshift could not be determined "YY.MM" References Ref Reference Code --- BibCode 19-digit reference code, as used in ADS, CDS and NED --- Authors List of authors --- Alan Wright Parkes Francois Ochsenbein CDS 1996 May 10 UNKNOWN UNKNOWN The original Parkes radio catalogue was compiled from major radio surveys with the Parkes radiotelescope at frequencies of 408 MHz and 2700 MHz. This work spanned a period of nearly 20 years and was undertaken largely by John Bolton and his colleagues. Since then, improved positions, optical identifications and redshifts have been obtained for many of the sources in the Catalogue. Furthermore, flux densities at several frequencies have supplemented the original surveys so that the measurements now cover the frequency range 80 - 22,000 MHz. However coverage at the highest frequencies is still sparse. Important contributions to the usefulness of the catalogue have been radio data from the Molonglo 408 MHz survey and the 80 MHz Culgoora measurements of Slee et al. PKSCAT90 should thus be regarded as a compendium of radio and optical data about southern radiosources. However, at the moment, it contains only sources originally found in the Parkes 2700 MHz Survey (see e.g. Part 14, Bolton et al, 1979, Aust J Phys, Astrophys Suppl, No. 46 and references therein) The original radio survey data of the Catalogue and the optical identifications have been published in a series of papers in the Australian Journal of Physics (see above reference). The associated optical spectral data on which redshifts were obtained has also been published, mainly in Astrophysical Journal and Monthly Notices of the Royal Astronomical Society. About the completeness levels of the Catalogue in various parts of the sky: users should note that the sky zone between -4 and +4 degrees has been the subject of a re-survey and is now complete to 0.25 Jy. About PKSCAT90: The PKSCAT90 database is made available for astronomical research purposes at a cost of $40.00 to cover the cost of floppy disks, packing and postage. However we request that users acknowledge their use of the catalogue data in publications as: Parkes Catalogue, 1990, Australia Telescope National Facility The New Version Of The Catalogue: This catalogue differs in several important ways from the older (VAX/VMS only) version (which we shall refer to as "PKSCAT85") in that: 1. It has a different and more compact structure than PKSCAT85 and thus takes up less disc space. 2. It contains J2000 (FK5) positions and names. This is the IAU-preferred system. Generally the B1950 data is for convenience only and is given to a limited precision of 1 arcsec. 3. Improved positions for many sources have been included. Following the J2000 position is an explicit upper limit to the positional accuracy in arcsecs. 5. The new catalogue contains 8400MHz fluxes from recent Parkes measurements of around 1100 of the stronger sources. 6. References to identifications and redshifts are available for some sources in the catalogue. The codes placed after the J2000 position can be used to refer to sources in a table at the end of this information. Nomenclature Notes: In the past, Parkes source names have been given in a format similar to: 1934-638 Unfortunately this is inconsistent with the IAU recommendations as to nomenclature (see e.g. Dickel et al, 1987, A & A Suppl. 68, 75-80 or <http://cdsweb.u-strasbg.fr/iau-spec.html>) since: (i) it doesn't specify the Equinox and Equator (e.g. B1950 or J2000) of the position from which the name is derived and (ii) decimal fractions of degrees are not permitted in the "declination-part" of the name However, because they are so widely used, we have kept the existing nomenclature for all "1950-type" names, but include a B in front of them. The J2000 names are given as: J1229+0203 where the letter signifies J2000 equinox and equator (FK5-type position), the next 4 digits are the hours and minutes of right ascension and the sign and final digits are the degrees and minutes of declination. Thus, the source 3C273 in the new system will be referred to as: PKSB1226+023 or PKSJ1229+0203 if the observatory designation is important or, more informally, B1226+023 or J1229+0203 The latter style of naming has been adopted for the catalogue software. For the Future: In the future, the catalogue will be expanded to include extra information from: new radio surveys, new identifications, many more references, improved positions and variability of fluxes. Furthermore we propose to extend the coverage of the Catalogue northward of +27 degrees declination using data from the northern surveys so as eventually to produce an all-sky, "Master" radio catalogue. Most importantly, we would very much like to receive references to pre-print and published information which supersedes or augments data in the present catalogue. Please assist by sending such material to: Alan Wright & Robina Otrupcek, PKSCAT Project ATNF, Parkes P.O. Box 276 PARKES NSW 2870 Australia Alternatively we can be contacted by E-MAIL on: PKSCAT@ATPARKES.RP.CSIRO.AU Next, in addition to the IBM/ PC version, a mainframe version of PKSCAT90 is now available in VAX/VMS format together with suitable interrogation and report generating programs. We are also preparing an Apple Macintosh version of PKSCAT90 for those users who have access to the FileMaker database program. Distribution is planned for later this year. The handling and postage prices will be the same as for the PC version. Finally, we are preparing a Radio Atlas of the southern sky using data from the PKSCAT90 database. This will be in a similar format to the optical, "Norton's" star atlas and should be available by 1 August 1990. Alan Wright & Robina Otrupcek 10 May 1990 UNKNOWN UNKNOWN of the data files: * June 1993, corrections from H. Andernach (hja@vilspa.esa.es) a) The source B0000-177 is NOT 3C465 (but source B2335+267) b) The last source B0420-086 is misplaced In references: BE66b is AuJP 19, 275 (not p. 27) W67 is MN 135, p. 339 (not p. 24) * 10-May-1996: Alan Wright [Parkes], Francois Ochsenbein [CDS]: Documentation rewritten. * 10-Jul-1999: catalogue reformatted at CDS to allow an automatic recognition of all numeric fields (magnitude, redshift, flux densities) References were also reformatted, and the bibcodes were added. * 17-Jul-1999: The source B1246-410 was wrongly associated to NGC4296, corrected to NGC4696 (H. Andernach <heinz@astro.ugto.mx>) VIII_15.xml Molonglo Reference Catalogue of Radio Sources 8016 VIII/16 Molonglo Reference Catalogue of Radio Sources Molonglo Reference Catalogue of Radio Sources M I Large L E Cram A M Brugess The Observatory 111 72 1991 1991Obs...111...72L Radio sources " 408-MHz survey observations made with the Molonglo Radio Telescope have been used to prepare a catalogue of 12 141 discrete sources of listed flux density >= 0.7 Jy. The survey covers 7.85 sr of the sky defined by +18.5 (deg) >= dec(1950) >= -85.0 (deg), mod(b) >= 3 (deg). A few sources beyond the declination limits are also included. The catalogue comprises celestial coordinates with standard error typically lying between 3 and 10 arcsec and 408-MHz flux densities with standard error typically lying between 4 and 10 per cent. Galactic coordinates, notes on source morphology and cross-references to the Parkes Catalogues are included. The overall source density is 1500/sr, corresponding to 0.001 per beam area. There are 7347 sources of listed flux density >= 1.00 Jy, at which level the catalogue is substantially complete. The reliability is believed to be better than 99.9 per cent. " The MRC was re-issued in 1990 with the original B1950 coordinates supplemented by J2000 values, and an additional cross-reference flag `J' added to denote (extended) sources imaged at 843-MHz by P.A. Jones. No other alterations were made to the original release. The MRC is now available on 5.25 inch, 1.2 Mbyte MS-DOS (IBM) floppy disk (0.5 inch magnetic tape is also available, but is not the preferred medium). In the floppy disk format, simple software is provided to facilitate use of the catalogue on a PC computer.
Catalog Data Bname Recommended IAU name of the source based on B1950 equinox. The first four characters are the hours and minutes of right ascension, and the last four the signed declination in tenths of a degree (unrounded). Column 9 contains the letters A, B, etc. denoting sources having the same eight-character IAU designation but decreasing flux density. --- RAh Right ascension (hours) in B1950 equinox h RAm RA (minutes) in B1950 equinox min RAs RA (sec) in B1950 equinox s DE- Declination sign --- DEd DEC in degrees in B1950 equinox deg DEm DEC in arcminutes in B1950 equinox arcmin DEs DEC in arcseconds in B1950 equinox arcsec RAh2000 Right ascension (hours) in J2000 equinox (Converted from B1950 using the STARLINK program COCO) h RAm2000 RA (minutes) in J2000 equinox min RAs2000 RA (seconds) in J2000 equinox s DE-2000 Declination sign --- DEd2000 DEC in J2000 equinox deg DEm2000 DEC in J2000 equinox arcmin DEs2000 DEC in J2000 equinox arcsec e_RAs2000 Standard error in RA (in seconds of time) s flag1 '*' indicates that the values obtained from two or more independent transits are scattered more than expected. --- e_DEs2000 Standard error in Dec (in seconds of arc) arcsec flag2 See flag1 --- Flux Flux density Jy e_Flux Standard error Jy flag3 See flag1 --- Mflag Morphology flags Morphology flags blank - no clear evidence of departure from point A - Source with small-scale structure E - Extended source C - Complex extended source M - Multiple sources (within 8 arcmin of another) N - Weak neighbouring sources --- Cflag1 Cross-reference flag1 J - See Jones (1989) --- Cflag2 Cross-reference flag2 Cross-reference flag2 P - Source lies within 2 arcmin of a Parkes source T - Discussed in the original MNRAS MRC paper S - See Schilizzi and McAdam (1975) M - See Clarke et al. (1976) C - See Cameron (1971) R - See Robertson (1973) Two flags at most are used in Cols 75-76, with P>T>S>M>C>R. --- GLON Galactic longitude deg GLAT Galactic latitude deg C.-H. Joseph Lyu Hughes STX/NASA 1995 Aug 01 UNKNOWN UNKNOWN DATA STRUCTURE. The machine-readable MRC is provided as 12 141 ASCII records, each of fixed length 87 bytes (each followed by CR,LF). The first line is listed below, with `x' in positions that may be occupied by characters but are blank in the first record : =========================================================================== 1 10 20 30 40 50 | | | | | | 0000-506x 00 00 09.2 -50 41 31 00 02 42.5 -50 24 49x.3xx4xx 60 70 80 | | | xx1.28x.06xxxxxpx-64.9 321.4 =========================================================================== FORTRAN CODE TO READ MRC FORTRAN 77 source is included (MRC.FOR) to allow menu-driven reading of the MRC as provided here. The FORTRAN program is self-explanatory. It expects to find the MRC ASCII data file in the current directory and with the name MRCJ2000. An executable version of this FORTRAN code has been produced (using Microsoft FORTRAN Version 5, with a library which uses a co-processor should one be available) and may be invoked on an IBM AT or compatible by setting the correct current directory and typing `MRC'. The program will run faster if the source and data are placed on a hard disk. The original MRC was published in Mon. Not. R. astr. Soc., Vol 194, pp 693-704 and Microfiches MN 194/1. VIII_16.xml The 1.4-GHz Northern Sky Catalog 8017 VIII/17 31524 1.4-GHz Sources The 1.4-GHz Northern Sky Catalog R L White R H Becker ApJS 79 331 1992 1992ApJS Radio sources This catalog contains a list of 30239 1.4 GHz radio sources over the declination range of -5 degrees to 82 degrees. This catalog is based on the Green Bank 1.4 GHz Northern Sky Survey (Condon and Broderick 1985, 1986), which was generated using the Green Bank 300 foot (91m) telescope. The threshold for identifying a 1.4 GHz radio source was set at 100 mJy. The catalog data include the source name, a confusion flag, right ascension (1950), declination (1950), 1.4 GHz flux, a flag to indicate if the source is extended at 20 cm, 4.85 GHz flux (from Becker et al. 1991), a flag to indicate if the source is extended at 6 cm, 0.365 GHz flux (from Douglas et al. 1980), spectral index between 6 and 20 cm, and spectral index between 20 and 80 cm. Where possible, the source name is derived from the 6 cm catalog of Becker et al. 1991.
Catalog Data NAME 20cm Name 20 cm Name, constructed from RA, Dec HHMM+DDMM with A or B added at end if needed to make name unique. When a 20cm source matches a sources in the 6cm catalog of Becker, White, & Edwards (1991, Ap J Supp 75, 1) the 6cm name and position (good to 40" at the 90% confidence level) are used. Sources without a 6cm counterpart have names ending in L; their positions are only accurate to 160" at the 90% confidence level). --- CONFLG flag ? indicates that a 20cm source matched more than one 6cm or 80cm source, so confusion is likely. In that case the additional matches are listed in following lines. --- RAh Hours of right ascension (1950) h RAm Minutes of RA min RAs Seconds of RA s DE- Sign of declination --- DEd Degrees of declination deg DEm Minutes of declination arcmin DEs Seconds of declination arcsec FLUX 1.4 GHz flux mJy EXTFLG "*" if source is extended at 20cm, else blank --- CFLUX 4.85 GHz flux from Becker et al (1991) mJy CEXTFLG "*" if source is extended at 6cm, else blank --- PFLUX 0.365 GHz flux from Texas survey, Douglas et al., private comm. mJy SpHI Spectral index between 6 and 20 cm; blank if not detected at 6 cm. F(nu) = C*nu**alpha. --- SpLO Spectral index between 20 and 80 cm; blank if not detected at 80cm --- C.-H. Joseph Lyu Hughes STX/NASA 1995 Aug 01 UNKNOWN UNKNOWN THE 1.4 GHZ NORTHERN SKY CATALOG - Distribution version, 4 December 1991 This is a brief description of the format of the distribution version of the 20 cm Northern Sky Catalog of White, R. L. and Becker, R. H. (1992, Ap.J.Supp., in press). For more details see the paper. The catalog is in an ascii file with 69 characters per record. It can be read with the following Fortran statements: character name*10, conflg, decsgn*1, extflg, cextflg integer rahh, ramm, decdd, decmm, decss, flux, cflux, pflux real rass, sihi, silo read(10,1) name, conflg, rahh, ramm, rass, & decsgn, decdd, decmm, decss, & flux, extflg, cflux, cextflg, pflux, sihi, silo 1 format(a10, 1x, a1, 1x, i2, 1x, i2, 1x, f4.1, 1x, & a1, i2, 1x, i2, 1x, i2, 1x, & i7, a1, 1x, i7, a1, 1x, i7, 1x, f4.1, 1x, f4.1) Note that several of the columns may be blank, so in an actual application one would have to be careful about zero values for a number of items. Here are a few sample lines from the catalog: 123456789 123456789 123456789 123456789 123456789 123456789 123456789 0000-0041 00 00 24.0 -00 41 17 167 139 432 -0.1 -0.7 0000+6849L 00 00 26.4 +68 49 39 721* 0000+1821 00 00 27.9 +18 21 39 123 177 299 0.3 -0.7 0000+5457 ? 00 00 28.6 +54 57 33 140 45 351 -0.9 -0.7 2359+5453 ? 23 59 25.3 +54 53 57 140 128 -0.1 0000+4600 00 00 31.6 +46 00 06 123 27 181 -1.2 -0.3 0000+5814 00 00 31.9 +58 14 56 329 104 1137 -0.9 -0.9 VIII_17.xml The 6C Survey of Radio Sources - I. Declination Zone Dec > 80 deg 8018 VIII/18 6C Survey of Radio Sources I The 6C Survey of Radio Sources - I. Declination Zone Dec > 80 deg J E Baldwin R C Boysen S E G Hales J E Jennings P C Waggett P J Warner Mon. Not. R. Astron. Soc. 217 717 1985 1985MNRAS Radio sources Surveys "The 6C Survey of Radio Sources - I. Declination Zone Dec > 80 deg" (6CSRSI) contains a compilation of radio source observations made with the use of an (non-tracking) Earth-rotation aperture synthesis telescope comprising many small aerial arrays on an east-west baseline operating at 151 MHz. This paper is the first in a series of papers giving radio source observations at 151 MHz. See the discussion in 6CSRSI for details on the design and operation of the telescope and the generation of the survey. The other papers in this series include, Hales et al. (1988), Hales et al. (1990) and Hales et al. (1991). This portion of the catalogue contains a listing of 1761 radio sources ordered by increasing right ascension. The survey covers a circular area of radius 10 deg centered on the North Celestial Pole. This survey has been divided into 32 separate maps. Flux densities are on the scale of Roger, Bridle, and Costain (1973) (RBC). The authors believe the flux density scale is consistent with the RBC scale to within +/-10%. Both the peak flux density and the integrated flux densities required a primary-beam correction, and the peak flux densities required a further correction for the reduction in peak brightness caused by chromatic aberration. The latter correction is dependent on the distance of the source from the field center. See 6CSRSI for details on source selection criterion, calibration, and error analysis. Source positions have been systematically adjusted with respect to a frame defined by standard positions of the 3C sources in the field. Positional uncertainties have been estimated to correspond to approximately 4 arcsec/S, where S is the apparent peak flux density (in Jy) before primary beam correction. See 6CSRSI for further details. Note that this file only contains the catalogue of radio sources. It is intended to be used with the radio maps originally published on microfiche in Baldwin, Boysen, Hales, Jennings, Waggett, Warner and Wilson (1985). The source lists and FITS format maps for the four regions of the 6C survey published to date have been placed on a CDROM entitled "Images from the Radio Universe", which is available from the address below. A nominal fee may be charged for such requests. Prof. Jim Condon NRAO Edgemont Road Charlottesville, Virginia 22903-2475 Structure: The File as a Whole "Survey of Radio Sources - I. Declination Zone Dec > 80 deg" consists of a single fixed-block file of 1761 36-byte records. The original file contained 40-byte records. Detailed descriptions of some of the fields in the file are given in the following sections. Catalog File Bytes Units Format Item 1 - 2 h I2 Right ascension (B1950) 4 - 5 m I2 Right ascension (B1950) 7 - 8 s I2 Right ascension (B1950) 10 - 12 deg I3 Declination (B1950) 14 - 15 arcmin I2 Declination (B1950) 17 - 18 arcsec I2 Declination (B1950) 21 - 25 Jy F5.2 Flux density (peak) 27 - 31 Jy F5.2 Flux density (integ.) 35 - 36 I2 Contour map panel Table 1: Catalog Record Format Flux density (peak): Source peak flux density at 151 MHz. Flux density (integrated): Source integrated flux density at 151 MHz. Integrated flux densities were carried out for sources with fitted peak flux densities above 300 mJy per beam area (before primary beam correction). The integration was carried out to a limiting level of 10% of the fitted peak (or 50 mJy for sources having fitted peak values <500 mJy. The sums were then normalized by comparison with the same procedure applied to an ideal point source of 1 Jy. Note that for unresolved sources the integrated flux value can fall below the peak value. If the column is blank the peak flux was not strong enough to calculate the integrated flux. Contour map panel: This column contains the number of the map panel in which the source appears. There are 32 panels in this survey. This catalogue contains the first section of the 6C Cambridge survey of radio sources at 151 MHz. This part of the survey covers the region north of a declination of 80 deg. This survey has an angular resolution of 4.2 arcmin x 4.2 arcmin x cosec(dec) (half-power at map center) and a limiting flux density of 120mJy at 151 MHz. Data include the source positions (B1950), peak flux density, integrated flux density, and contour map number. This part of the survey contains 1761 sources.
The 6C I Catalog RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec PeakFlux Flux density (peak) Jy IntFlux Flux density (integ.) Jy map_num Contour map panel --- 6csrsi.tex ADC LaTeX Document N.P.M. Kuin and N. Oliversen ADC/SSDOO/NASA 1995 May 10 UNKNOWN UNKNOWN "The 6C Survey of Radio Sources - I. Declination Zone Dec > 80 deg" was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Heinz Andernach. The catalog was originally submitted by the first author, Dr. Sally Hales. VIII_18.xml Catalogues from a deep 327 MHz Westerbork Survey 8019 VIII/19 Catalogues from a deep 327 MHz Westerbork Survey Catalogues from a deep 327 MHz Westerbork Survey M H Wieringa Bull. Inf. CDS 43 17 1993 1993BICDS..43...17W Radio sources Surveys We present the results of a deep survey of six fields with the Westerbork Synthesis Radio Telescope at 327 MHz. In total we have detected ~4500 sources brighter than our 5-sigma noise level, which ranges from 2.4-3.5 mJy/beam, over an area of ~95 square degrees. For four fields we also obtained 608 MHz observations, for the remaining two fields 608 MHz observations were already available. We present the source catalogues at both frequencies and derive source counts and spectral indices. The data were calibrated using the DWARF redundancy package and absolute calibration is based on 3C286, using a flux of 26.93 Jy at 327 Mhz and 21.47 Jy at 608 MHz. The source parameters were determined using a gaussian fitting procedure for all but the most complex sources and statistical corrections for noise bias were applied. As part of my PhD-thesis at Leiden Observatory I made the following surveys at 327 and 608 MHz using the Westerbork Synthesis Radio Telescope: -------------------------------------------------------------------------- 64W2: Lynx, 327 MHz only (this field has been mapped at this frequency before by M.J.A. Oort (thesis), I've added a 2 after the W to indicate the revised list), numbers do not correspond because the present survey is more sensitive. 69W : Draco, a survey of 2 overlapping fields at 327 MHz and 6 fields at 608 MHz. 70W : Umi, 327 MHz only, one field. 75W : OH471, one 327 MHz field and three 608 MHz fields 76W : Cam, one 327 MHz field and three 608 MHz fields -------------------------------------------------------------------------- Sources detected at both frequencies have corresponding numbers in the 327 MHz (92cm) and 608 MHz (50cm) lists. Multiple sources are indicated by a '*' after the name, their components by 'A','B', etc. Components of multiple sources do not necessarily correspond between the two frequencies, also in some cases one or more components may not be detected at the other frequency. The .tex files are in plain TeX format The .dat files were written with the following format (fortran): FORMAT(A8,1X,F9.2,1X,F4.2,1X,F9.1,1X,F4.1,1X,F8.2,1X,F7.2,1X,A2, 1 1X,F5.1,1X,F4.1,1X,F4.0,1X,F3.0,1X,F5.1,1X,F5.2,1X,F7.2, 1 1X,F5.2,1X,F5.2)
Survey 64W2, 327 MHz (in Lynx) Survey 69W, 608MHz (in Draco) Survey 69W, 327MHz (in Draco) Survey 70W, 327MHz (in UMi) Survey 75W, 608MHz (OH 471) Survey 75W, 327MHz (OH 471) Survey 76W, 608MHz (in Cam) Survey 76W, 327MHz (in Cam) NAME Westerbork survey name + source number number=1 The NAME has the form nnWmmmmM, where nn is Westerbork survey number, mmmm the source sequence number and M is blank for single sources, '*' for multiples, 'A', 'B', 'C',... for components --- RAh Right Ascension B1950 (hours) number= -1.0 indicates an undefined mean error h RAm Right Ascension B1950 (minutes) number= -1.0 indicates an undefined mean error min RAs Right Ascension B1950 (seconds) number= -1.0 indicates an undefined mean error s e_RAs Mean error on RA number= -1.0 indicates an undefined mean error s DE- Declination B1950 (sign) number= -1.0 indicates an undefined mean error --- DEd Declination B1950 (degrees) number= -1.0 indicates an undefined mean error deg DEm Declination B1950 (minutes) number= -1.0 indicates an undefined mean error arcmin DEs Declination B1950 (seconds) number= -1.0 indicates an undefined mean error arcsec e_DEs Mean error on DE number= -1.0 indicates an undefined mean error arcsec S Flux density at: 327 MHz for *92cm.dat files 608 MHz for *50cm.dat files number= -1.0 indicates an undefined mean error mJy e_S Mean error on S number= -1.0 indicates an undefined mean error mJy Res indicates whether the source is unresolved (2) resolved (R, fitted gaussian parameters follow), extended (E, multiple components found and given on subsequent lines) number= -1.0 indicates an undefined mean error --- l_MajAxis '<' indicates that an estimated upper limit to the size follows (for Unresolved sources) number= -1.0 indicates an undefined mean error --- MajAxis The major axis (FWHM) of the fitted gaussian (for resolved sources) or maximum component separation (for extended sources) number=2 The 'Res' flag takes the values 'U' when the source is unresolved; in this case, the values of MajAxis, PA and MinAxis (as well as their mean errors) should be ignored (see the *.tex files) 'R' when the source is resolved; in this case, the fitted gaussian parameters follow 'E' for extended source; multiple components are found and given on subsequent lines. arcsec e_MajAxis =-1.0 Mean error on MajAxis -1.0 indicates an undefined mean error number= -1.0 indicates an undefined mean error arcsec PA Position angle (North through East)(2) number= -1.0 indicates an undefined mean error deg e_PA Mean error in PA number=2 The 'Res' flag takes the values 'U' when the source is unresolved; in this case, the values of MajAxis, PA and MinAxis (as well as their mean errors) should be ignored (see the *.tex files) 'R' when the source is resolved; in this case, the fitted gaussian parameters follow 'E' for extended source; multiple components are found and given on subsequent lines. deg MinAxis The minor axis (FWHM, arcsec) of the fitted gaussian number=2 The 'Res' flag takes the values 'U' when the source is unresolved; in this case, the values of MajAxis, PA and MinAxis (as well as their mean errors) should be ignored (see the *.tex files) 'R' when the source is resolved; in this case, the fitted gaussian parameters follow 'E' for extended source; multiple components are found and given on subsequent lines. arcsec R Ratio of total flux to fitted peak flux number= -1.0 indicates an undefined mean error --- SN Peak signal to noise ratio of source in map number= -1.0 indicates an undefined mean error --- Atten Primary beam attenuation (>1) number= -1.0 indicates an undefined mean error --- W Statistical weight for use in source counts number= -1.0 indicates an undefined mean error --- 64w92cm.tex Survey 64W2, 327MHz, plain TeX version 69w50cm.tex Survey 69W, 608MHz, plain TeX version 69w92cm.tex Survey 69W, 327MHz, plain TeX version 70w92cm.tex Survey 70W, 327MHz, plain TeX version 75w50cm.tex Survey 75W, 608MHz, plain TeX version 75w92cm.tex Survey 75W, 327MHz, plain TeX version 76w50cm.tex Survey 76W, 608MHz, plain TeX version 76w92cm.tex Survey 76W, 327MHz, plain TeX version CDS 1994 Sep 20 UNKNOWN UNKNOWN *09-Jul-1993: First version of this Description file; *20-Sep-1994: Second version, Notes have been added, verified against the Standards VIII_19.xml A Catalogue of 5 GHz Galactic Plane Sources 8020 VIII/20 Cat of 5 GHz Galactic Plane Sources A Catalogue of 5 GHz Galactic Plane Sources R F Haynes J L Caswell L W J Simons Aust. J. Phys. Astrophys. Suppl 48 1 1979 1979AuJPA..48....1H Galactic plane Radio sources This is a catalog of 915 sources in the galactic plane between l=190 - 360 - 40 for -2 < b < 2. The l, b pair of galactic coordinates is given in columns 1 and 2 and essentially constitutes the galactic source name. The 1950 equatorial coordinates for each source are given in columns 3 and 4, and values for the peak brightness temperature and flux density are given in columns 5 and 6. The reader should refer to Section 3 of the source reference for information relating to the determination of the flux densities. Column 7 gives an estimate of the source extension in minutes of arc. Extents are given for source in nonconfused regions only. Finally, in column 8 comments on each source are included where appropriate. Identifications with known supernova remnants are included from the compilation of Clark and Caswell (1976). Identifications with HII regions are based principally on H109alpha recombination-line emission data, which are mostly obtained from Wilson et al. (1970) but with some unpublished Parkes observations included also.
915 radio sources in the galactic plane GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Tb Peak brightness temperature K S Flux density The source flux densities given in table1 were determined by estimating the mean of the beam brightness temperatures at the four points spaced at one-half of the half-power beamwidth from each nominal source position. The quoted flux density is double the difference between this mean and the peak observed source brightness (with appropriate scaling, that is x1.3, from beam temperature to janskys). In the calculation, the assumption was made that the source is a point source. This technique results in a good estimate for point sources even where there are several nearby sources or a confused background. However, many of the sources are clearly extended. We have not attempt to estimate integrated flux densities for these objects; thus the catalogued flux densities are correct only for those apparently 'point-like' radio sources. We strongly urge that the catalogue be used only in close conjunction with the maps; they alone can provide an adequate description of complex regions. The angular size, when quoted in the table, refers to the full width of the source measured in the galactic longitude and latitude directions. It is intended only as a rough indication for sources much broader than the beam size; in very confused regions no attempt was made to assess the sizes of component sources. Jy dim1 Extent (first dimension) or dim1 arcmin x 'x' for dim1 x dim2 --- dim2 Extent (second dimension) or dim2 arcmin Com Identification Comment Identifications with known supernova remnants (SNR) from the compilation of Clark and Caswell (1976); identifications with HII regions mostly from Wilson et al. (1970). Abbreviations- C = Compact; E = Extended; PA= Part. --- M.J.Wagner, F. Ochsenbein CDS C.-H. Lyu Hughes STX/NASA 1996 Apr 08 The original CDS documentation by M.J. Wagner, F. Ochsenbein (1993) was included in this ReadMe file. UNKNOWN UNKNOWN The detection of sources from the survey maps was made using an automatic search routine with the CSIRO Cyber 76 computing system. Maps were held using the NOD-2 format (see Haslam 1974,1975) in machine readable form. Each map was systematically searched for sources above the background level equivalent to a main beam brightness temperature of 0.4 K. The initial search for sources consisted of identifying those grid points in the map which exceed the mean of the four adjacent surrounding points by a nominal 0.1 K (grid point are at the Nyquist sample interval). Subsequently, the 'rough' position and flux density were refined by a source-fitting technique. The fitting procedure involved using a 16-point beam, function, where the appropriate weighting for each grid point permitted the program to interpolate to the best position for the peak of the source while taking into account nearby galactic features. The beam-fitting procedure was used either side (alternating between right ascension and declination) of the nominal position to obtain the best estimate of the position of each source. The resulting positions have an accuracy comparable to the overall positional accuracy of the survey (30" arc). Peak main beam brightness temperatures (determined by fitting the 16-point beam response function at the deduced nominal position) are also accurate to within the survey accuracy. Sources with a peak beam brightness temperature of at least 0.2 K above the background are included, except in confused regions; a point source of 0.2 K corresponds to 0.26 Jy. VIII_20.xml The 6C Survey of Radio Sources - II. The Zone 30 Degrees < Dec < 51 Degrees, 09h 30m < RA < 17h 30m 8021 VIII/21 6C Survey of Radio Sources II The 6C Survey of Radio Sources - II. The Zone 30 Degrees < Dec < 51 Degrees, 09h 30m < RA < 17h 30m S E G Hales J E Baldwin P J Warner Mon. Not. R. Astron. Soc. 234 919 1988 1988MNRAS Radio sources Surveys "The 6C Survey of Radio Sources - II. The Zone 30 deg. < Dec < 51 deg., 08h 30m < RA < 17h 30m" (6CSRSII) contains a compilation of radio source observations made with the use of an (non- tracking) Earth-rotation aperture synthesis telescope comprising many small aerial arrays on an east-west baseline operating at 151 MHz. This paper is the second in a series: Details on the design and operation of the telescope and the reduction of the survey were first discussed in Baldwin et al. (1985). The third paper in this series was published in Hales et al. (1990) and the fourth paper in the series was published in Hales et al. (1991). The catalogue contains a listing of 8278 radio sources ordered by increasing right ascension from 8h 30m to 17h 30m . The survey is centered on a declination of 41 deg and includes from declination 30 deg to 50 deg. Five fields have been included in this survey: 0940+41, 1120+41, 1300+41, 1440+41, and 1620+41. Attenuation corrections were applied to all flux densities and maps using tables derived for each synthesis. Flux densities are on the scale of Roger, Bridle, and Costain (1973) (RBC). The authors believe the flux density scale is consistent with the RBC scale to within +/-5%. See 6CSRSII for details on source selection criterion and error analysis. Source positions have been systematically adjusted (by 0.6s in right ascension and by up to 10 arcsec in declination) to agree with known positions of bright sources. The residual rms scatter in the corrected positions of the reference sources relative to their true positions is estimated to be +/- 4 to 5 arcsec in each coordinate. See 6CSRSII for details. Note that this file only contains the catalogue of radio sources. It is intended to be used with the radio maps originally published on microfiche in Hales, Baldwin and Warner (1988). The source lists and FITS format maps for the four regions of the 6C survey published t-date have been placed on a CDROM entitled "Images from the Radio Universe", which is available from the address below. A nominal fee may be charged for such requests. Prof. Jim Condon NRAO Edgemont Road Charlottesville, Virginia 22903-2475 Structure: The File as a Whole "The 6C Survey of Radio Sources - II. The Zone 30 deg < Dec <51 deg, 08h 30m < RA < 17h 30m "consists of a single fixed-block file of 8278 50-byte records. The original file contained 80-byte records. Detailed descriptions of some of the fields in the file are given in the following sections. This catalogue contains the second section of the 6C Cambridge survey of radio sources at 151 MHz, covering the region from 30 deg to 51 deg in declination and between 8h 30m and 17h 30m in right ascension. The survey has an angular resolution of 4.2 arcmin x 4.2 arcmin x cosec(dec). Data include the source positions (B1950), peak flux density, integrated flux density, contour map panel number and contour map field names. Its limiting flux density depends weakly on right ascension and strongly on declination and is 190 mJy in the central part of the declination strip but rises to over 400 mJy near its northern and southern boundaries. This part of the survey contains 8278 sources, covering an area of 2030 square degrees.
Catalog Data RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec PeakFlux Flux density (peak) Flux density (peak): Source peak flux density at 151 MHz. Jy IntFlux Flux density (integ.) Flux density (integrated): Source integrated flux density at 151 MHz. Integrated flux densities were carried out for sources with apparent flux densities above 483 mJy. The integration was carried out to a limiting level of 10% of the fitted peak (or for 103 mJy for sources having apparent flux densities < 1.03 Jy). Note that for unresolved sources the integrated flux value can fall below the peak value. Jy n_IntFlux Integrated Flux flag Integrated flux flag: If the column is marked with a dash (-), the peak flux was not strong enough to calculate the integrated flux. If the column is marked with an asterisk (*), the peak flux was strong enough to qualify for integration, but it has been integrated into a brighter adjoining peak. --- map_num Contour map panel number Contour map panel number: This column contains the panel number of the contour map in which the source appears in the survey. Each map field is divided into 32 contour panels. The panel number and the map field name tell the user where to look up the source of interest in the published contour map. --- field Contour map field name Contour map field name: This column contains the name of the field in which the source appears. There are five fields in this survey: 0940+41, 1120+41, 1300+41, 1440+41, and 1620+41. The panel number and the map field name tell the user where to look up the source of interest in the published contour map. -------------------------------------------------------------------------------- Remarks and Modifications: "The 6C Survey of Radio Sources - II. The Zone 30 deg < Dec <51 deg, 08h 30m < RA < 17h 30m " was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Heinz Andernach. The catalog was originally submitted by the first author, Dr. Sally Hales. The integrated flux flag column was added by the ADC/CDS by extracting the character information from the Integrated flux density column. This was done to avoid mixing character and numeric information in the same column. --- 6csrsii.tex LaTeX Document N. A. Oliversen and N.P.M. Kuin ADC/SSDOO/NASA 1995 May 10 VIII_21.xml The 6C Survey of Radio Sources - III. The Zone 48 Degrees < Dec < 68 Degrees, 05h 25m < RA < 18h 17m 8022 VIII/22 6C Survey of Radio Sources III The 6C Survey of Radio Sources - III. The Zone 48 Degrees < Dec < 68 Degrees, 05h 25m < RA < 18h 17m S E G Hales C R Masson P J Warner J E Baldwin Mon. Not. R. Astron. Soc. 246 256 1990 1990MNRAS Radio sources Surveys "The 6C Survey of Radio Sources - III. The Zone 48 deg < Dec <68 deg, 05h 25m < RA < 18h 17m" (6CSRSIII) contains a compilation of radio source observations made with the use of an (non- tracking Earth-rotation aperture synthesis telescope comprising many small aerial arrays on an east-west baseline operating at 151 MHz. This paper is the third in a series of papers giving radio source observations at 151 MHz. See the discussion in Baldwin et al. (1985) for details on the design and operation of the telescope and the generation of the survey. Other papers in this series include Hales et al. (1988) and Hales et al. (1991). This portion of the catalogue contains a listing of 8749 radio sources ordered by increasing right ascension. The survey is centered on a declination of 58 deg to facilitate calibration using Cassiopea A. This survey has been divided into six separate fields with up to 32 panels per field. Flux densities are on the scale of Roger, Bridle, and Costain (1973) (RBC). The authors believe the flux density scale is consistent with the RBC scale to within +/-5%. Both the peak flux density and the integrated flux densities required a primary-beam correction, and the peak flux densities required a further correction for the reduction in peak brightness caused by chromatic aberration. The latter correction is dependent on the distance of the source from the field center. See 6CSRSIII and Hales et al. (1988) for details on source selection criterion, calibration, and error analysis. Source positions have been adjusted by 1.1s to 2.3s in right ascension and up to -40 arcsec in declination, to agree with known positions of bright sources. The authors believe that the residual systematic errors are less than +/-5 arcsec in each coordinate. Note that this file only contains the catalogue of radio sources. It is intended to be used with the radio maps originally published on microfiche in Hales, Masson, Warner and Baldwin (1990). The source lists and FITS format maps for the four regions of the 6C survey published to date have been placed on a CDROM entitled "Images from the Radio Universe", which is available from the address below. A nominal fee may be charged for such requests. Prof. Jim Condon NRAO Edgemont Road Charlottesville, Virginia 22903-2475 Structure: The File as a Whole "The 6C Survey of Radio Sources - III. The Zone 48 deg < Dec < 68 deg , 05h 25m < RA < 18h 17m " consists of a single fixed-block file of 8749 48-byte records. The original file contained 51-byte records. Detailed descriptions of some of the fields in the file are given in the following sections. This catalogue contains the third section of the 6C Cambridge survey of radio sources at 151 MHz. This part of the survey covers the region from 48 deg to 68 deg in declination and between 5h 25m and 18h 17m in right ascension. This survey has an angular resolution of 4.2 arcmin x 4.2 arcmin x cosec(dec) (half-power at map center). The limiting flux density varies between 160 mJy to 600 mJy as a function of map and declination. Data include the source positions (B1950), peak flux density, integrated flux density, contour map panel number and contour map field names. This part of the survey contains 8749 sources, covering an area of 1950 square degrees. This catalogue slightly overlaps the Hales et al. (1988) survey.
Catalog data RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec PeakFlux Flux density (peak) Flux density (peak): Source peak flux density at 151 MHz. Jy IntFlux Flux density (integ.) Flux density (integrated): Source integrated flux density at 151 MHz. Integrated flux densities were carried out for sources with fitted peak flux densities above 456 mJy per beam area (before primary beam correction). The integration was carried out to a limiting level of 10% of the fitted peak (or 98 mJy for sources having fitted peak values <0.98 Jy). Note that for unresolved sources the integrated flux value can fall below the peak value. Jy n_IntFlux Integrated flux flag Integrated flux flag: If the column is marked with a dash (-), the peak flux was not strong enough to calculate the integrated flux. If the column is marked with an asterisk (*), the peak flux was strong enough to qualify for integration, but it has been integrated into a brighter adjoining peak. --- map_num Contour map panel number Contour map panel number: This column contains the name of the map panel in which the source appears. There are up to 32 panels per map field in this survey. The panel number and map field name tell the user where to look up the source of interest in the published contour map. A panel number listed with a negative sign indicates that the data are accommodated at the location but come from another map or area of sky. --- colon The character ":" --- field Contour map field name Contour map field name: This column contains the name of the field in which the source appears. Six fields have been included in this survey: 0700+58, 0900+58, 1100+58, 1300+58, 1500+58, and 1700+58. The panel number and map field name tell the user where to look up the source of interest in the published contour map. -------------------------------------------------------------------------------- Remarks and Modifications: "The 6C Survey of Radio Sources - III. The Zone 48 deg < Dec <68 deg, 05h 25m < RA < 18h 17m" was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Heinz Andernach. The catalog was originally submitted by the first author, Dr. Sally Hales. The integrated flux flag column was added by the ADC/CDS by extracting the character information from the Integrated flux density column. This was done to avoid mixing character and numeric information in the same column. --- 6csrsiii.tex LaTeX ADC Document N. Oliversen and N.P.M. kuin ADC/SSDOO/NASA 1995 May 10 VIII_22.xml The 6C Survey of Radio Sources - IV. The Zone 67 Degrees < Dec < 82 Degrees, 0h < RA < 24h 8023 VIII/23 6C Survey of Radio Sources IV The 6C Survey of Radio Sources - IV. The Zone 67 Degrees < Dec < 82 Degrees, 0h < RA < 24h S E G Hales C J Mayer P J Warner J E Baldwin Mon. Not. R. Astron. Soc. 251 46 1991 1991MNRAS Radio sources Surveys "The 6C Survey of Radio Sources - IV. The Zone 67 deg < Dec < 82 deg, 0h < RA < 24h" (6CSRSIV) contains a compilation of radio source oservations made with the use of an (non-tracking) Earth- rotation aperture synthesis telescope comprising many small aerial arrays on an east-west baseline operating at 151 MHz. This paper is the fourth in a series: Details on the design and operation of the telescope and the reduction of the survey were first discussed in Baldwin et al. (1985). Other papers in the series include Hales et al. (1988) and Hales et al. (1990). The present zone overlaps that covered in Baldwin et al. (1985) over the range 80 deg < Dec < 82 deg and also that covered in Hales et al. (1990) over the range 67 deg < Dec < 68 deg and 5h 25m < RA < 18h 17m. The catalogue contains a listing of 5421 radio sources ordered by increasing right ascension from 0h to 24h. The survey is centered on a declination of 75 deg and includes from declination 67 deg to 82 deg. Eight fields have been included in this survey: 0100+75, 0400+75, 0700+75, 1000+75, 1300+75, 1600+75, 1900+75, and 2200+75. Attenuation corrections were applied to all flux densities and maps using tables derived for each synthesis (see Hales et al. 1988). Flux densities are on the scale of Roger, Bridle and Costain (1973) (RBC). The authors believe the flux density scale is consistent with the RBC scale to within +/-5%. See 6CSRSIV and Baldwin et al. (1985) for details on source selection criterion and error analysis. Source positions have been adjusted (by 2.8s to 5.5s in right ascension and by up to 1100 in declination) to agree with known positions of bright sources. The residual rms scatter in the corrected positions of the reference sources relative to their true positions is estimated to be +/- 3 to 5 arcsec in each coordinate. See 6CSRSIV for details. Note that this file only contains the catalogue of radio sources. It is intended to be used with the radio maps originally published on microfiche in Hales, Mayer, Warner and Baldwin (1991). The source lists and FITS format maps for the four regions of the 6C survey published to date have been placed on a CDROM entitled "Images from the Radio Universe", which is available from the address below. A nominal fee may be charged for such requests. Prof. Jim Condon NRAO Edgemont Road Charlottesville, Virginia 22903-2475 Structure: The File as a Whole "The 6C Survey of Radio Sources - IV. The Zone 67 deg < Dec < 82 deg, 0h < RA < 24h " consists of a single fixed-block file of 5421 50-byte records. The original file was variable format with 49-bytes per record. Detailed descriptions of some of the fields in the file are given in the following sections. This catalogue contains the fourth section of the 6C Cambridge survey of radio sources at 151 MHz, covering the region from 67 deg to 82 deg in declination and between 0h and 24h in right ascension. The survey has an angular resolution of 4.2 arcmin x 4.2 arcmin x cosec(dec). Data include the source positions (B1950), peak flux density, integrated flux density, contour map panel number and contour map field names. The limiting flux density is 160 mJy at 151 MHz in the present zone with completeness achieved at 400 mJy on the best maps and at about 800 mJy on the worst. This part of the survey contains 5421 sources, covering an area of 1440 square degrees.
Catalog Data RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec PeakFlux Flux density (peak) Flux density (peak): Source peak flux density at 151 MHz. Jy IntFlux Flux density (integ.) Flux density (integrated): Source integrated flux density at 151 MHz. Integrated flux densities were carried out for sources with apparent flux densities above 513 mJy. The integration was carried out to a limiting level of 10% of the fitted peak (or for 110 mJy for sources having apparent flux densities < 1.10 Jy). For the right-half of the field 1900+75, the threshold to qualify for integration was raised to 1.54 Jy and for the apex of the field 2200+75, to 0.96 Jy, with limiting level for both cases of 10% (or 154 mJy for sources having apparent peak flux densities < 1.54 Jy). Note that for unresolved sources the integrated flux value can fall below the peak value. Jy n_IntFlux Integrated flux flag Integrated flux flag: If the column is marked with a dash (-), the peak flux was not strong enough to calculate the integrated flux. If the column is marked with an asterisk (*), the peak flux was strong enough to qualify for integration, but it has been integrated into a brighter adjoining peak. --- map_num Contour map panel number Contour map panel number: This column contains the panel number of the contour map in which the source appears in the survey. The number of contour panels per map field varies from 27 to 32. The panel number and the map field name tell the user where to look up the source of interest in the published contour map. --- colon The character ":" --- field Contour map field name Contour map field name: This column contains the name of the field in which the source appears. Eight fields have been included in this survey: 0100+75, 0400+75, 0700+75, 1000+75, 1300+75, 1600+75, 1900+75, and 2200+75. The panel number and the map field name tell the user where to look up the source of interest in the published contour map. -------------------------------------------------------------------------------- Remarks and Modifications: "The 6C Survey of Radio Sources - IV. The Zone 67 deg < Dec < 82 deg, 0h < RA < 24h " was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Heinz Andernach. The catalog was originally submitted by the first author, Dr. Sally Hales. The integrated flux flag column was added by the ADC/CDS by extracting the character information from the Integrated flux density column. This was done to avoid mixing character and numeric information in the same column. --- 6csrsiv.tex LaTeX Document N. Oliversen and N.P.M. Kuin ADC/SSDOO/NASA 1995 May 10 VIII_23.xml The 6C Survey of Radio Sources - V. The Zones 6C-Va (48 deg < Dec < 68 deg, 01h 34m < RA < 06h 14m., 6C-Vb (48 deg < Dec < 68 deg, 17h 16m < RA < 20h 24m) 8024 VIII/24 6C Survey of Radio Sources V The 6C Survey of Radio Sources - V. The Zones 6C-Va (48 deg < Dec < 68 deg, 01h 34m < RA < 06h 14m., 6C-Vb (48 deg < Dec < 68 deg, 17h 16m < RA < 20h 24m) S E G Hales C R Masson P J Warner J E Baldwin D A Green Mon.Not.R.Astron.Soc. 262 1057 1993 1993MNRAS.262.1057H Radio sources Surveys "The 6C Survey of Radio Sources - V. The Zones 6C-Va (48 deg < Dec < 68 deg, 01h 34m < RA < 06h 14m) and 6C-Vb (48 deg < Dec < 68 deg, 17h 16m < RA < 20h 24m )" (6CV) contains a compilation of radio source observations made with the use of an (non-tracking) Earth-rotation aperture synthesis telescope comprising many small aerial arrays on an east-west baseline operating at 151 MHz. This paper is the fifth in a series of papers giving radio source observations at 151 MHz. See the discussion in 6CI (Baldwin et al. 1985) for details on the design and operation of the telescope and the initial generation of the survey. Other papers in this series include 6CII (Hales et al. 1988), 6CIII (Hales et al. 1990), 6CIV (Hales et al. 1991), and 6CVI (Hales et al. 1993b). The 6CV catalog contains a total listing of 3458 radio sources ordered by increasing right ascension. The survey is centered on a declination of 58 deg to facilitate calibration using Cassiopeia A. The 6CVa covers the region 48 deg < Dec < 68 deg , 01h 34m < RA < 06h 14m, and the 6CVb covers 48 deg < Dec < 68 deg , 17h 16m < RA < 20h 24m . Both of the 6CV regions have some overlap in right ascension with the 6CIII catalog so that 396 sources have alternative entries in both catalogs. In addition, there is some overlap with the 6CIV paper in this series. Positional calibration was effected as for 6CIII (Hales et al. 1990) and give corrections of similar magnitude. Flux densities are on the scale of Roger et al. (1973). Provisional flux densities were corrected for the measured receiver gain at a declination of 58 deg as a function of right ascension. The final flux densities were adjusted to be consistent with published radio source lists and were adjusted for consistency with overlapping regions in the 6CIII, 6CIV, and the 6CVI catalogs. See 6CV for additional flux calibration details. Note that these two sections of the 6CV submitted to the ADC contain only the listing of radio sources and not the radio maps. The radio source lists are intended to be used with the radio maps originally published on microfiche in Hales, Masson, Warner, Baldwin, and Green (1993). Structure: The File as a Whole "The 6C Survey of Radio Sources - V. The Zones 6C-Va (48 deg < Dec < 68 deg, 01h 34m < RA < 06h 14m) and 6C-Vb (48 deg < Dec < 68 deg, 17h 16m < RA < 20h 24m)" consists of two fixed-block files. The 6CVa consists of 2229 52-byte records, and the 6CVb consists of 1229 52-byte records. Descriptions of some of the fields in the file are given in the following section. The record format is the same for the 6CVa and 6CVb. This catalog contains the fifth section of the 6C Cambridge survey of radio sources at 151 MHz (6CV). This part of the survey covers two regions: 48 deg < Dec < 68 deg, 01h 34m < RA < 06h 14m [6CVa] and 48 deg < Dec < 68 deg, 17h 16m < RA < 20h 24m [6CVb]. The limiting flux density is generally 170 mJy. The catalog data include the source positions (B1950), peak flux density, integrated flux density, contour map panel number, contour map field names, and integrated flux flag. The two regions together list a total of 3458 sources (2229 in 6CVa and 1229 sources in 6CVb). The 6CV catalog consists of two files: one file contains the 6CVa, and the second file contains the 6CVb. records.
The 6C Va catalog The 6C Vb catalog RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec PeakFlux Flux density (peak) Flux density (peak): Source peak flux density at 151 MHz. Jy IntFlux Flux density (integrated) Flux density (integrated): Source integrated flux density at 151 MHz. Jy map_num Contour map panel number Contour map panel number: This column contains the name of the map panel in which the source appears. The panel number and map field name tell the user where to look up the source of interest in the published contour map. Typically, each map is divided into 32 panels, although the 0300+58 map contains panel numbers up to 36, presumably from an adjoining region (see Figure 4 in 6CV). A panel number listed with a negative sign indicates that the data are accommodated at the location but come from another map or area of sky. --- field Contour map field name Contour map field names: This column contains the name of the field in which the source appears. Three fields have been included in this survey: 0300+58, 0500+58 for 6CVa and 1900+58 for 6CVb. The panel number and map field name tell the user where to look up the source of interest in the published contour map. --- n_IntFlux Integrated_flux_flag Integrated flux flag: A dash (-) indicates that the peak flux was not strong enough to calculate the integrated flux. An asterisk (*) indicates that the peak flux was strong enough to qualify for integration, but it has been integrated into a brighter adjoining peak. -------------------------------------------------------------------------------- Remarks and Modifications: "The 6C Survey of Radio Sources - V. The Zones 6C-Va (48 deg < Dec < 68 deg, 01h 34m < RA < 06h 14m) and 6C-Vb (48 deg < Dec < 68 deg, 17h 16m < RA < 20h 24m)" was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Heinz Andernach. The catalog was originally submitted by Dr. Sally Hales. The integrated flux flag column was generated by the ADC by editing the original integrated flux field and moving the character flags to a separate column. This was done to avoid the mixing of characters and numbers in a single field. --- 6csrsv.tex ADC Documentation Nancy Oliversen and Paul Kuin ADC 1995 May 11 VIII_24.xml The 6C Survey of Radio Sources - VI. The Continuous Zone 30 deg < Dec < 51 deg, 00h < RA < 09h 05m and 22h 35m < RA < 24h 8025 VIII/25 6C Survey of Radio Sources VI The 6C Survey of Radio Sources - VI. The Continuous Zone 30 deg < Dec < 51 deg, 00h < RA < 09h 05m and 22h 35m < RA < 24h S E G Hales J E Baldwin P J Warner Mon.Not.R.Astron.Soc. 263 25 1993 1993MNRAS.263...25H Radio sources Surveys The 6C Survey of Radio Sources - VI. The Continuous Zone 30 deg < Dec < 51 deg , 00h < RA < 09h 05m and 22h 35m < RA < 24h (6CVI) contains a compilation of radio source observations made with the use of an (non-tracking) Earth-rotation aperture synthesis telescope comprising many small aerial arrays on an east-west baseline operating at 151 MHz. This paper is the sixth in a series of papers giving radio source observations at 151 MHz. See the discussion in 6CI (Baldwin et al. 1985) for details on the design and operation of the telescope and the initial generation of the survey. Other papers in this series include 6CII (Hales et al. 1988), 6CIII (Hales et al. 1990), 6CIV (Hales et al. 1991), and 6CV (Hales et al. 1993a). The 6CVI catalog contains a total listing of 6752 radio sources ordered by increasing right ascension. The 6CVI covers the region 30 deg < Dec < 51 deg , 00h < RA < 09h 05m and 22h 35m < RA < 24h. This survey has been divided into six fields with up to 32 panels per field. The 6CVI has some overlap in right ascension with the 6CII catalog so that 199 sources have alternative entries in both catalogs. In addition, there is some overlap with the 6CIII and 6CV papers in this series. Positional calibration was effected as for 6CII except that a separate constant right ascension correction was obtained for each map as well as a separate declination correction varying linearly with declination. The right ascension correction ranged from 0.18 sec to 0.79 sec, and the most severe declination correction reached -25". Flux densities are on the scale of Roger et al. (1973). Provisional flux densities were corrected for the measured receiver gain at a declination of 41 deg as a function of right ascension. The final flux densities were adjusted to be consistent with the radio sources in other published radio source lists and were adjusted for consistency with overlapping regions in the 6CIII, 6CV catalogs. See 6CVI for additional flux calibration details and for source selection criteria. Note that this ADC catalog contains only the radio source list and does not include the radio maps. The radio source list is intended to be used with the radio maps originally published on microfiche in Hales, Baldwin, and Warner (1993). Structure: The File as a Whole The 6C Survey of Radio Sources - VI. The Continuous Zone 30 deg < Dec < 51 deg, 00h < RA < 09h 05m and 22h 35m < RA < 24h consists of a single fixed-block file consisting of 6752 52-byte records. Descriptions of some of the fields in the file are given in the following section. This catalog contains the sixth section of the 6C Cambridge survey of radio sources at 151 MHz (6CVI). This part of the survey covers the region 30 deg < Dec < 51 deg, 00h < RA < 09h 05m and 22h 35m < RA < 24h. The catalog data include the source positions (B1950), peak flux density, integrated flux density, contour map panel number, contour map field names, and an integrated flux flag. This catalog contains a list of 6752 sources in 2440 square degrees.
Catalog Data RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec PeakFlux Flux density (peak) Flux density (peak): Source peak flux density at 151 MHz. Jy IntFlux Flux density (integrated) Flux density (integrated): Source integrated flux density at 151 MHz. Integrated flux densities were derived for sources with apparent flux densities above 1 Jy (2 Jy for the top panels of the map 2340+41 to avoid severe runaway problems). See 6CVI for further details on generation of the source list. Jy map_num Contour map panel number Contour map panel number: This column contains the name of the map panel in which the source appears. The panel number and map field name tell the user where to look up the source of interest in the published contour map. Each map is divided into 32 panels. A panel number listed with a negative sign indicates that the data are accommodated at the location but come from another map or area of sky. --- field Contour map field name Contour map field names: This column contains the name of the field in which the source appears. Six fields have been included in this survey: 2340+41, 0120+41, 0300+41, 0440+41, 0620+41, and 0800+41. The panel number and map field name tell the user where to look up the source of interest in the published contour map. --- n_IntFlux Integrated_flux_flag Integrated flux flag: A dash (-) indicates that the peak flux was not strong enough to calculate the integrated flux. An asterisk (*) indicates that the peak flux was strong enough to qualify for integration, but it has been integrated into a brighter adjoining peak. -------------------------------------------------------------------------------- Remarks and Modifications: The 6C Survey of Radio Sources - VI. The Continuous Zone 30 deg < Dec < 51 deg , 00h < RA < 09h 05m and 22h 35m < RA < 24h was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Heinz Andernach. The catalog was originally submitted by the first author, Dr. Sally Hales. The integrated flux flag column was generated by the ADC by editing the original integrated flux field and moving the character flags to a separate column. This was done to avoid the mixing of characters and numbers in a single field. --- 6csrsvi.tex LaTeX ADC Documentation Nancy Oliversen and Paul Kuin ADC 1995 May 11 VIII_25.xml Results of a Five-year Program of Multifrequency Monitoring of Low-frequency Variable Radio Sources 8026 VIII/26 Low-frequency Variable Radio Sources Results of a Five-year Program of Multifrequency Monitoring of Low-frequency Variable Radio Sources K J Mitchell B K Dennison J J Condon D R Altschuler H E Payne S L O'Dell J J Broderick Astrophys. Journ. Suppl. 93 441 1994 1994ApJS...93..441M Nonstellar objects Radio sources QSOs X-ray sources The Lowvar dataset is the result of a detailed multi-frequency monitoring program of 34 low-frequency variable radio sources. This consists of flux density measurements at five frequencies between 0.3 GHz and 1.4 GHz over the five year period, 1980.0 - 1985.0. The sources monitored were previously found to be variable or probably variable in two- and three-epoch observations at 318 MHz of complete samples of extragalactic sources. Observations were carried out at 318, 430 and 606 MHz using the National Astronomy and Ionosphere Center Arecibo 305-m radio telescope and at 880 and 1400 MHz using the National Radio Astronomy Observatory Green Bank 91-m radio telescope. The measured flux densities and their errors are given according to source, frequency and date. The measurement error is sufficiently small that variations larger than several percent can be identified. The errors do not reflect time-independent uncertainties in absolute scale and therefore absolute comparison with other measurements is not possible with high accuracy. The Lowvar dataset is expected to be useful for studies of radio source variability caused by both extrinsic and intrinsic mechanisms, and for studies comparing variations at different wavebands. Partial results of these observations on selected sources were reported by Payne et al. (1982), Altschuler et al. (1984), Dennison et al. (1984a), and Dennison et al. (1984b). The complete results (tabulated in the accompanying data set) and the observations are described in detail by Mitchell et al. (1993).
Catalog Data ID Source Name --- FreqCode Frequency Code Frequency Code - 1 for 318 MHz; 2 for 430 MHz; 3 for 606 MHz 4 for 880 MHz; 5 for 1400 MHz. --- Obs_yr Date of Observation - 1900 yr Obs_m Date of Observation - Month --- Obs_d Date of Observation - Day d Flux Flux Density Jy e_Flux Flux Density Error Jy C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 08 The original ADC documentation by Brian Dennison (1994) was used to create this ReadMe file. UNKNOWN UNKNOWN The source 0723-00 is suspected of having a large scale error at 430 MHz, owing to the large zenith angle (19.5 deg) used at that frequency, which is near the Arecibo telescope limit. This source is included, however, as real and significant variability is clearly present at all frequencies, including 430 MHz. VIII_26.xml The Bell Laboratories H I Survey 8028 VIII/28 Bell Laboratories H I Survey The Bell Laboratories H I Survey A A Stark C F Gammie R W Wilson J Bally R A Linke Astrophys. J. Suppl. 79 77 1992 1992ApJS...79...77S H I data Interstellar medium Surveys The sky north of declination -40 deg. was observed in the 21 cm line of atomic hydrogen with the FWHM = 2 deg. beam of the 20 foot horn reflector at AT&T Bell Laboratories, Crawford Hill. The survey covers a velocity range of 654 km/s centered on the Galactic standard of rest, with 5.3 km/s wide filters. This survey is distinguished by its sensitivity to low surface brightness features (antenna temperature about 50 mK) and relative freedom from sidelobe contamination. High-velocity clouds are extracted and cataloged automatically. The data are presented in declination zones in equatorial and polar coordinates, and as R.A. - velocity images.
Observations were made as drift scans along even declinations between -40 deg. and +90 deg. at the epoch (1981) of the observations. The horn antenna has a FWHM beam size of 2 deg. at 21 cm. This large beam made it possible to cover the whole visible sky in 66 constant declination scans. The survey is undersampled in declination (one beam width sampling) and oversampled in right ascension (roughly quarter beamwidth sampling). The average rms noise of spectra taken at all declinations is 0.017 K in 5.2 km/s wide channels, although in some cases baseline problems make the survey unreliable at this level. The survey contains 19,248 spectra. The data are in FITS format.
whsky1.fit Whole Sky Image T*dV -365, -355 whsky2.fit Whole Sky Image T*dV -360, -350 whsky3.fit Whole Sky Image T*dV -355, -345 whsky4.fit Whole Sky Image T*dV -350, -340 whsky5.fit Whole Sky Image T*dV -345, -335 whsky6.fit Whole Sky Image T*dV -340, -330 whsky7.fit Whole Sky Image T*dV -335, -325 whsky8.fit Whole Sky Image T*dV -230, -320 whsky9.fit Whole Sky Image whsky10.fit Whole Sky Image whsky11.fit Whole Sky Image whsky12.fit Whole Sky Image whsky13.fit Whole Sky Image whsky14.fit Whole Sky Image whsky15.fit Whole Sky Image whsky16.fit Whole Sky Image whsky17.fit Whole Sky Image whsky18.fit Whole Sky Image whsky19.fit Whole Sky Image whsky20.fit Whole Sky Image whsky21.fit Whole Sky Image whsky22.fit Whole Sky Image whsky23.fit Whole Sky Image whsky24.fit Whole Sky Image whsky25.fit Whole Sky Image whsky26.fit Whole Sky Image whsky27.fit Whole Sky Image whsky28.fit Whole Sky Image whsky29.fit Whole Sky Image whsky30.fit Whole Sky Image whsky31.fit Whole Sky Image whsky32.fit 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npcap70.fit North Polar Cap Image T*dV -20, -10 npcap71.fit North Polar Cap Image T*dV -15, -5 npcap72.fit North Polar Cap Image T*dV -10, 0 npcap73.fit North Polar Cap Image T*dV -5, 5 npcap74.fit North Polar Cap Image T*dV 0, 10 npcap75.fit North Polar Cap Image T*dV 5, 15 npcap76.fit North Polar Cap Image npcap77.fit North Polar Cap Image npcap78.fit North Polar Cap Image npcap79.fit North Polar Cap Image npcap80.fit North Polar Cap Image npcap81.fit North Polar Cap Image npcap82.fit North Polar Cap Image npcap83.fit North Polar Cap Image npcap84.fit North Polar Cap Image npcap85.fit North Polar Cap Image npcap86.fit North Polar Cap Image npcap87.fit North Polar Cap Image npcap88.fit North Polar Cap Image npcap89.fit North Polar Cap Image npcap90.fit North Polar Cap Image npcap91.fit North Polar Cap Image npcap92.fit North Polar Cap Image npcap93.fit North Polar Cap Image npcap94.fit North Polar Cap Image npcap95.fit North Polar Cap Image npcap96.fit North Polar Cap Image 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spcap145.fit South Polar Cap Image T*dV 355, 365 ravel1.fit R.A. - Velocity Images SURVEY DEC = -40 ravel2.fit R.A. - Velocity Images SURVEY DEC = -38 ravel3.fit R.A. - Velocity Images -36 ravel4.fit R.A. - Velocity Images ravel5.fit R.A. - Velocity Images ravel6.fit R.A. - Velocity Images ravel7.fit R.A. - Velocity Images ravel8.fit R.A. - Velocity Images ravel9.fit R.A. - Velocity Images ravel10.fit R.A. - Velocity Images ravel11.fit R.A. - Velocity Images ravel12.fit R.A. - Velocity Images ravel13.fit R.A. - Velocity Images ravel14.fit R.A. - Velocity Images ravel15.fit R.A. - Velocity Images ravel16.fit R.A. - Velocity Images ravel17.fit R.A. - Velocity Images SURVEY DEC = -8 ravel18.fit R.A. - Velocity Images ravel19.fit R.A. - Velocity Images ravel20.fit R.A. - Velocity Images ravel21.fit R.A. - Velocity Images SURVEY DEC = 0 ravel22.fit R.A. - Velocity Images ravel23.fit R.A. - Velocity Images ravel24.fit R.A. - Velocity Images ravel25.fit R.A. - Velocity Images SURVEY DEC = 8 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Velocity Images ravel55.fit R.A. - Velocity Images ravel56.fit R.A. - Velocity Images ravel57.fit R.A. - Velocity Images ravel58.fit R.A. - Velocity Images ravel59.fit R.A. - Velocity Images ravel60.fit R.A. - Velocity Images ravel61.fit R.A. - Velocity Images ravel62.fit R.A. - Velocity Images ravel63.fit R.A. - Velocity Images ravel64.fit R.A. - Velocity Images ravel65.fit R.A. - Velocity Images ravel66.fit R.A. - Velocity Images SURVEY DEC = 90 N. G. Roman and N.P.M. Kuin NASA/SSDOO/ADC 1995 Apr 11 UNKNOWN UNKNOWN The file names from the tape were renamed to distighuish the different coordinate systems and projections easily. In the notes some information from the HISTORY records in the FITS headers was appended. The data were read with the FITS routines from the IDL ASTRONOMY USER'S LIBRARY maintained by Wayne Landsman (Landsman@stars.gsfc.nasa.gov). VIII_28.xml A 1400-MHz Survey of 1478 Abell Clusters of Galaxies 8029 VIII/29 1400-MHz Survey of 1478 Abell Clusters of Galaxies A 1400-MHz Survey of 1478 Abell Clusters of Galaxies F N Owen R A White K C Hilldrup R J Hanisch Astron. Journ. 87 1083 1982 1982AJ.....87.1083O Radio sources Galaxies, radio Clusters, galaxy Surveys This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974). The primary goals of this survey were to observe all Abell (1958) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness GE 3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10 GE 17.0; richness LE 2). This dataset contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published version has 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.
1400-MHz survey of Abell Clusters ID Abell cluster number An asterisk by the Abell cluster number in ID means only that the cluster is outside of Abell's galactic latitude limits for completeness. --- Rich Richness class Richness 0 clusters need not have an asterisk. --- Dist Distance class --- m10 ]0,] Magnitude of tenth brightest galaxy mag zest ]0,] Redshift (z) estimate The redshift was estimated using using the method of Corwin (1974) including a richness correction. --- Radius ]0,] Corrected Abell cluster radius arcmin RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s e_RAs ]0,] Error in right ascension s DE- Declination: sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec e_DEs ]0,] Error in declination arcsec S1400 ]0,] Total flux density at 1400 MHz Jy e_S1400 ]0,] Flux density error at 1400 MHz Jy MajAxi [0,] Deconvolved major axis length These columns contain entries for sources not included in Owen (1974) or for sources with new measurements. arcmin e_MajAxi ]0,] Major axis error arcmin n_MajAxi Major axis note For sources from Owen et al. (1974) a resolution code is given; NR (not significantly resolved or less than 5 arcmin), A (5-10 arcmin), B (10-15 arcmin), C (greater than 15 arcmin). These values refer to the source sizes after deconvolution with the telescope beam. --- MinAxi [0,] Deconvolved minor axis arcmin e_MinAxi ]0,] Minor axis error arcmin n_MinAxi Minor axis note --- PA [0,360[ Position angle deg e_PA ]0,] Position angle error deg dist-C ]0,] Distance from cluster center Ratio of the distance of the source from the cluster center to the corrected Abell cluster radius. pc N.A.Oliversen ADC H.Andernach CDS C.-H.Lyu Hughes STX 1996 Apr 08 This catalog was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Heinz Andernach. The data were originally received by H. Andernach, on tape, from R. J. Hanisch in 1984. The original ADC and CDS documentation by N.A. Oliversen and H. Andernach (1994) was used to create this ReadMe file. In column n_MinAxi the last record shows a value of 77, which is unexplained. UNKNOWN UNKNOWN The original data (2 lines per source and higher accuracy parameters) were reformatted by Dr. Andernach, to one line per source, and truncated to the published, significant digits. Moreover, the sources were sorted by B1950 coordinates, not by Abell cluster number as in the original publication. Information on whether the cluster is in Abell's statistical sample was not contained in the data file from Hanisch, but can be recovered e.g. from Struble and Rood (1987) (cf. NASA ADC catalog A7096). Two additional columns (n_MajAxi, n_MinAxi) were added to the ADC version of this catalog by extracting the character fields from the original MajAxi and MinAxi columns, in order to avoid mixing numeric and character fields in the same columns. VIII_29.xml The 5C14, 5C15, and 5C16 Radio Source Surveys of the 5C12 Area 8030 VIII/30 5C14/5C15/5C16 Radio Survey at 408 and 1407 MHz The 5C14, 5C15, and 5C16 Radio Source Surveys of the 5C12 Area C R Benn S Kenderdine Mon. Not. Roy. Astron. Soc. 251 253 1991 1991MNRAS.251..253B Galactic pole, north Radio sources Surveys This catalog contains the fourteenth, fifteenth, and sixteenth sections of the 5C Cambridge survey of radio sources. This catalog reports further 408 and 1407 MHz observations of the 5C12 area (Benn et al. 1982), which were carried out with the One-Mile Telescope at Cambridge to provide more accurate positions for the 5C12 sources and to extend the 5C12 catalog. Positions and flux densities were measured for 691 sources in a 5 degree x 5 degree area near the north galactic pole. The catalog data include the serial (source) number, right ascension (B1950.0) and declination (B1950.0), rms uncertainty in 408 MHz position, peak 408 MHz flux density and rms uncertainty, effective envelope attenuation (P_eff) at 408 MHz, difference between the 408 MHz and 1407 MHz positions, rms uncertainty in 1407 MHz position, peak 1407 MHz flux density and uncertainty, envelope attenuation P at 1407 MHz and radio spectral index between 408 MHz and 1407 MHz.
Catalog Data ID Source name The serial number of the 5C12 source is given in this column. Additions to the 316-source catalog given in Benn et al. 1982 are numbered from 5C12.317 onwards. Pairs of 1407 MHz detections blended at 408 MHz are numbered as one source with components a, b. Sources 5C12.7 and 5C12.9 of 5C12 are now known to be lobes of a wide double (see Section 2 of Benn et al. 1988), and here they have been numbered 7a and 7b. --- RAh Right ascension (B1950) Right ascension, declination: The coordinates have been corrected for precession to epoch B1950.0 measured at 408 MHz or, if detected at the higher frequency only, at 1407 MHz. The positions are weighted means of those measured from the 5C12 and 5C14 + 15 + 16 maps. h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- sign of Declination --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec ErRA408 Rms uncertainty in the 408 MHz R.A. Rms uncertainty in the 408 MHz right ascension. The uncertainty in declination is larger by a factor cosec (declination), approximately 1.74 at the 5C12 map center. arcsec S408 Peak 408 MHz flux density Peak 408 MHz flux density and rms uncertainty, measured from the 5C14 + 5C15 + 5C16 combined map. Flux densities are on the scale of Kellermann et al. (1969); to bring them on to the scale of Baars et al. (1977), they should be multiplied by 1.07 (Riley 1988). mJy e_S408 Rms uncertainty in S408 mJy Att-408 Effective envelope attenuation at 408 MHz Effective envelope attenuation P_eff at 408 MHz. S408 must be multiplied by this factor to recover the apparent flux density S' with which the source appears on the 5C14 + 5C15 + 5C16 map, and hence the signal-to-noise ratio. --- Diff-ra RA difference in between 408 and 1407 MHz Difference between 408 MHz and 1407 MHz positions in the sense 1407-408 MHz. The 1407 MHz position was measured from whichever of the 5C12, 5C14, 5C15, or 5C16 maps gave the highest signal-to-noise ratio. arcsec Diff-dec DEC difference in between 408 and 1407 MHz arcsec ErRA1407 Rms uncertainty in the 1407 MHz R.A. Rms uncertainty in 1407 MHz right ascension. The uncertainty in declination is larger by a factor cosec(declination). arcsec S1407 Peak 1407 MHz flux density Peak 1407 MHz flux density and uncertainty. The flux density was measured from whichever of the 5C12, 5C14, 5C15, or 5C16 maps gave the highest signal-to-noise ratio. Flux densities are on the scale of Kellermann et al. (1969); to bring them on to the scale of Baars et al. (1977), they should be multiplied by 1.04. mJy e_S1407 Rms uncertainty in S1407 mJy Att-1407 Effective envelope attenuation at 1407 MHz --- Alpha Radio Spectral Index Radio spectral index between 408 and 1407 MHz, defined by S_nu =~ nu^(alpha). --- C.-H. Joseph Lyu Hughes STX/NASA 1996 Apr 08 The original ADC documentation by N. A. Oliversen (1994) was used to create this ReadMe file. UNKNOWN UNKNOWN The 5C14, 5C15, and 5C16 Radio Source Surveys of the 5C12 Area was received by the Astronomical Data Center (ADC), NASA Goddard Space Flight Center, from Dr. Heinz Andernach. The catalog was originally submitted to Dr. Andernach by Dr. C. Benn. The "alpha" or spectral index column differed in sign between the published version of this catalog and the electronic version submitted to the ADC. Apparently the absolute value of the column was the same in the two versions, only the sign was affected. The electronic version was modified by the ADC to agree with the printed catalog. The declination (seconds) column contained a mix of I2 and F4.1 format numbers in the electronic version submitted to the ADC. A decimal point was added to the I2 format numbers (byte number 29) by the ADC so the entire column could be read with an F4.1 format. No change was made to the data values themselves. VIII_30.xml A revised machine-readable source list for the Rees 38-MHz survey. 8031 VIII/31 Revised source list for the Rees 38-MHz survey A revised machine-readable source list for the Rees 38-MHz survey. S E G Hales E M Waldram N Rees P J Warner Mon. Not. R. Astron. Soc. 274 447 1995 1995MNRAS.274..447H A revised machine-readable source list for the Rees 38-MHz survey. N Rees Mon. Not. R. Astron. Soc. 244 233 1990 1990MNRAS.244..233R Radio sources Surveys Atlases We present a revised machine-readable source list for the Rees 38-MHz (or '8C') survey with improved positions and no redundancy. The Rees 38-MHz survey covers an area of about 1 sr north of declination +60 degrees. The angular resolution is 4.5 x 4.5cosec(dec) arcmin**2 and the limiting flux density over much of the survey area is about 1 Jy. Both of these figures are an improvement by nearly an order of magnitude on previous surveys at this frequency. Users of these data should consult and cite the original survey paper by Rees as primary reference (=1990MNRAS.244..233R) with the present publication (=1995MNRAS.submitted) as a supplementary revision. The recommended style of reference is thus : "The revised Rees 38-MHz survey (Rees 1990, catalogue revised Hales et. al 1995)." Note that for interest the source list includes data on some sources at declinations lower than +60 degrees, but that the right ascension coverage is not complete below +60 degrees.
38-MHz data on 5859 sources RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (arcminutes) arcmin DEs Declination B1950 (arcseconds) arcsec SType Source type P = Simple source with only one local maximum within the source region (defined by the contour which encircles the local maximum and is 2.5 times the local noise level). The position is that of the peak flux brightness. C = Component or source associated with a single local maximum within an integrated complex. The peak and integrated flux for each such component represent values for that component only, and the position is that of the peak brightness. The components of a complex are not grouped together in the revised list, because it is ordered in right ascension. --- PEAK Peak brightness (Jy/beam) Peak brightness of source or component, measured in Jy/(beam area). The area of the synthesised beam is 4.5 x 4.5cosec(dec) arcmin**2. --- INTEG Integrated flux density (Jy) Integrated flux density of source or component. Jy Size Size (integrated area/synth beam) This is an indicator of the extent of the source and is the ratio of the integration area of the source to the area of a synthesised beam, calculated using the same integration level. Thus, size = 1 indicates a point source, size < 1 indicates some over-resolution due to noise effects, and size > 1 an apparently extended source. Most sources appear slightly extended because of distortions created by the ionosphere. Remember that the survey is confusion limited! --- SigNo Signal-to-noise ratio of detection The signal-to-noise, ie: the ratio of the peak brightness to the local noise level calculated at the position of the source. The revised list contains only sources or components with signal-to-noise >= 5.0. It excludes the components with signal-to-noise < 5.0 listed in Rees 1990 for some complexes. --- AtlasNum Number of contour plot in Rees 1990 This gives the number of the contour plot on which the source appears in the atlas provided in Rees 1990, to enable the user to check the appearance and environment of the source. The atlas may be obtained in preprint form - see paper for details. --- Sally Hales Cambridge, UK 1994 Nov 30 UNKNOWN UNKNOWN Discussion of the units used for peak brightness: The beam is not of constant size, the resolution being 4.5 x 4.5cosec(dec) arcmin**2. The point of quoting the peak brightness in Jy/beam is that, for a source which is not significantly resolved or distorted by ionospheric effects, the peak brightness in those units will give a reasonable estimate of the flux density of the source (and be numerically comparable to the integrated flux density in Jy). The provided on size also ties in with this idea by comparing the integration area of a source to the area of a synthesised beam. The original paper by Rees contains much discussion about the relative merits of peak brightness and integrated flux density as estimates of a source flux density, including consideration of the behaviour of their ratio ; all this hinges on the idea of flux being smeared out w.r.t. the theoretical synthesised beam, so that the concept of a beam area is crucial to the discussion. VIII_31.xml A study of spectral characteristics of the RC-Catalog and preliminary optical identifications. 8033 VIII/33 Spectral characteristics of RATAN A study of spectral characteristics of the RC-Catalog and preliminary optical identifications. N N Bursov N E Gol'neva N M Lipovka N S Soboleva A V Temirova Soobshch. Spets. Astrof. Obs. 63 50 1989 1989SoSAO..63...50B J/A+AS/87/1 : The RATAN-600 7.6 cm catalog (Parijskij et al, 1991) 1 Amirhanyan V.R., et al. (1989), Separata, Moscow Univ. 2 Bennet C.L., Lawrence C.R., Burke B.F., Hewitt J.N. =1986ApJS...61....1B 3 Lawrence C.R., Bennet C.L., Garcia-Baretta J.A., Greenfield P.E., Burke B.F., =1983ApJS...51...67L 4 Hunstead R.W., 1972, MNRAS 157, 367 5 Preston R.A., Morabito D.D., Williams J.G., Faulkner D.L., Jancey D.L., Nicolson G.D., =1985AJ.....90.1599P 6 Large M.I., Mills B.Y., Little A.G., Crawford D.F., Sutton J.M., =1981MNRAS.194..693L 7 Morabito D.D., Preston R.A., Slade M.A., Jauncey D.L., 1982, AJ 87, 517 8 Sharp J.R., Bash F.N., =1975AJ.....80..335S 9 Witzel A., Johnston K.J., 1982, Abs. Hamburger Sternw. 10, 151 10 Singal A.K., =1987A&AS...69...91S 11 Lawrence C.R., Bennet C.L., Hewitt J.N., Langston B.I., Klotz S.E., Burke B.F., Turner K.C., =1986ApJS...61..105L 12 Bettoni D., Buson L.M. =1987A&AS...67..341B 13 Hewitt A., Burbidge G., =1980ApJS...43...57H 14 Amirchanyan V.R., et al., 1985, Soobshch. Spets. Astrof. Obs. 47, 5 15 Wall J.V., Peacock J.A., =1985MNRAS.216..173W 16 Imke P., Weiler K.W., =1982MNRAS.198..747I 17 Weiler K.W., Johnston K.J., =1980MNRAS.190..269W 18 Walter H.G., West R.M., =1986A&A...156....1W 19 Adam G., =1985A&AS...61..225A 20 Barton R., Cappellaro E., Ciatti F., Turatto M., Kowal C.T., =1984A&AS...58..735B 21 Amirkhanian V.R., Gorshkov A.G., Ipatov A.V., Soobshch. Spets. Astrof. Obs. =1988SoSAO..58...41A 22 Schimmins A.J., Bolton J.G., 1972, Austral. J. Phys., Astrophys. Suppl. 23, 41 23 Torres C., Wroblewski H., =1987A&AS...69...23T 24 Dixon R.S., 1970 (Catalog <VII/2>) =1970ApJS...20....1D 25 Ehman J.R., Dixon R.S., Ramakrishna C.M., Kraus J.D., =1974AJ.....79..144E 26 Waldthausen H., Haslam C.G., Wielebinski R., Kronberg P.P., =1979A&AS...36..237W 27 Webb J.R., Smith A.G., Leacock R.J., Fitzgibbons G.L., Gombola P.P., Shepherd D.W., =1988AJ.....95..374W 28 Fitch L.T., Dixon R.S., Kraus J.D., =1969AJ.....74..612F 29 Wills J., 1975, Austral. J. Phys., Astrophys. Suppl. 38, 1 30 Veron-Cetty M.P., =1984A&AS...58..665V 31 Shectman S.A., =1985ApJS...57...77S 32 Sandage A., Bedke J., =1985AJ.....90.2006S" 33 Hintzen P., Ulvestad J., Owen F., =1983AJ.....88..709H 34 Schimmins A.J., Bolton J.G., Wall J.V., 1975, Austral. J. Phys., Astrophys. Suppl. 34, 63 35 Slee O.B., 1977, Austral. J. Phys., Astrophys. Suppl. 43, 1 36 Bolton J.G., Trett J., 1981, Austral. J. Phys., Astrophys. Suppl. 34, 445 37 Schimmins A.J., Bolton J.G., 1981, Austral. J. Phys., Astrophys. Suppl. 34, 471 38 Munro R.E.B., 1972, Austral. J. Phys., Astrophys. Suppl. 22, 1 39 Vitkovsky V.V., et al., 1984, Preprint N. 12 40 Ulvestad J., Johnston K., Perley R., Fomalont E.A., =1981AJ.....86.1010U 41 Bridle A.H., Davis M.M., Fomalont E.B., =1972AJ.....77..405B 42 Jauncey D.L., Hunstead R.W., =1972AJ.....77..345J 43 Stull M.A., =1971AJ.....76....1S 44 Stull M.A., =1973AJ.....78..285S 45 Kapahi V.K., Joshi M.N., Subrahmanya C.R., Gopal K., =1973AJ.....78..673K 46 Kellerman K.J., Pauliny-Toth I.I.K., =1973AJ.....78..828K 47 Ghigo F.D., Owen F., =1973AJ.....78..848G 48 Pauliny-Toth I.I.K., Kellerman K.J., =1972AJ.....77..797P 49 Vilebinsky V.V., et al., 1987, Tallin Obs. 50 Lipovka N.M., 1986, preprint SAO 51 Pauliny-Toth I.I.K., Wade C.M., Heeschen D.S., =1966ApJS...13...65P 52 Veron-Cetty M.P., Veron P., =1983A&AS...53..219V (Catalog <VII/54>) 53 Amirkhanyan V.R. (private comm.) 54 Slee O.B., Higgins C.S., 1973, =1973AuJPS..27....1S Austral. J. Phys., Astrophys. Suppl. 27, 1 55 Singal A.K., Gopal-Krishna, Steppe H., =1980MNRAS.191..581S 56 Readhead A.C.S., Hewish A., 1974, Mem. R. Astron. Soc. 78, 1 57 Gower J.F.R., Scott P.F., Wills D., 1967, Mem. R. Astron. Soc. 71, 49 =1967MmRAS..71...49G 58 Binette L., Carignan C., Bolton J.B., Wright A.E., 1981, Austral. J. Phys., Astrophys. Suppl. 34, 407 59 Galt J.A., Kennedy J.E.D., =1968AJ.....73..135G 60 Douglas J. (private comm.) 61 Fomalont E.B., 1967, Publ. Owens Valley, Calif. Inst. Technology, Pasadena, Vol.1, N.3 62 Golombek D., Miley G.K., Neugebauer G., =1988AJ.....95...26G 63 Hoskins, Murdoch H.S., Hazard C., Jauncey D.L., 1972, Austral. J. Phys., Astrophys. Suppl. 25, 559 RC Ratan Catalogue Radio sources The spectral analysis of the RC-catalog of the experiment "Cold" containing 840 radiosources in the interval of right ascension 4-22h are made. 280 spectra of radiosources are presented; 215 spectra are new. The mean spectral index for 196 objects with steep spectra (alpha >= 0 5) and flux densities >12mJy is 0.87+/-0.01. The preliminary optical identification of radiosources with catalogued galaxies is done.
List of Sources and Spectral indexes Name Name of Source: RC, J2000-based position; "t" stands for "twin" objects --- alpha Spectral index (S prop. to nu**(-alpha)) --- Radio fluxes Name Name of Source: RC, J2000-based position; "t" stands for "twin" objects --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s e_RAs Mean error on RAs s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec e_DEs Mean error on DEs arcsec nu Frequency of observation MHz l_S(nu) Limit flag on S(nu) --- S(nu) Flux density mJy e_S(nu) Mean error on Flux density mJy r_S(nu) Reference (see "References" section) --- Optical identifications Name Name of Source: RC, J2000-based position; "t" stands for "twin" objects --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s e_RAs Mean error on RAs s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec e_DEs Mean error on DEs arcsec Obj Optical identification number=1 the following abbreviations are used: Q = QSO ; G,E = Galaxy ; B = Blue object ; ST = Stellar-like object ; CG = Compact Galaxy. --- Mag Magnitude of the optical counterpart mag r_Obj Reference (see "References" section) --- James Marcout, Francois Ochsenbein CDS 1995 Dec 15 UNKNOWN UNKNOWN * 15-Dec-1995 : The catalog was created by J. Marcout at CDS in November 1995 from the paper publication. Several errors in the original reference list have been corrected. VIII_33.xml The Parkes Half-Jansky Flat-Spectrum Sample 8034 VIII/34 Parkes Half-Jansky Flat-Spectrum Sample The Parkes Half-Jansky Flat-Spectrum Sample M J Drinkwater R L Webster P J Francis J J Condon S L Ellison D L Jauncey J Lovell B A Peterson A Savage Mon. Not. R. Astron. Soc. 284 85 1997 1997MNRAS.284...85D VIII/5 : Bright Extragalactic Radio Sources (1Jy) (Kuehr+, 1981) VIII/15 : Parkes Radio Sources Catalogue (PKSCAT90) (Wright+ 1990) http://www.phys.unsw.edu.au/~mjd/papers : original papers Radio sources catalogs BL Lacertae objects: general galaxies: general quasars: general radio: continuum: galaxies We present a new sample of Parkes half-Jansky flat-spectrum radio sources having made a particular effort to find any previously unidentified sources. The sample contains 323 sources selected according to a flux limit of 0.5 Jy at 2.7 GHz, a spectral index measured between 2.7 and 5.0 GHz of {alpha}(2.7/5.0) > -0.5, where S(f) is proportional to f^alpha^, Galactic latitude |b| > 20{deg} and -45{deg} < Declination(B1950) < +10{deg}. The sample was selected from a region 3.90 steradians in area. We have obtained accurate radio positions for all the unresolved sources in this sample and combined these with accurate optical positions from digitised photographic sky survey data to check all the optical identifications. We report new identifications based on R- and Kn-band imaging and new spectroscopic measurements of many of the sources. We present a catalogue of the 323 sources of which 321 now have identified optical counterparts and 277 have measured spectral redshifts.
Parkes Half-Jansky Flat-Spectrum Sample (Table 5 of the paper) Seq Running number --- Name PKSCAT90 name (B1950) from cat. <VIII/15> --- S2.7 Flux density at 2.7GHz Jy S5.0 Flux density at 5.0GHz Jy alpha spectral index --- rFlux Flux reference --- RAh Right ascension B1950 (hours) h RAm Right ascension B1950 (minutes) min RAs Right ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec rPos position reference --- comment comment on radio/optical morphology number=1 a brief description of the radio morphology if the source is resolved using the terminology by Downes et al. (1986MNRAS.218...31D): P : partially resolved source Do : double sources with no central component Do+CC : double sources with a central component or peak H : diffuse halo around a central source HT : complex head-tail morphology Comments in parentheses refer to the optical identification. In cases where there was no match to the sky catalogues but the source was identified using CCD data, these are indicated as (B) (R) (I) and (K) for the respective wavebands. If the CCD imaging did not identify the source, the comment 'blank' is made, and 'STAR' indicates a source too near a bright star. If the source was confused with a close neighbour in the sky catalogues, but separated by a CCD image, the comment 'merge' is made followed by the waveband used; in some cases the Digitized Sky Survey data was used to separate the object ('DSS') --- dRA (optical-radio) RA offset arcsec dDE (optical-radio) Dec offset arcsec dr total position offset arcsec cl morphological classification number=2 g = galaxy, s = stellar, f = too faint, m = merged --- Bj Magnitude at optical Bj mag l_z (for lower limits) --- z redshift --- r_z redshift reference --- Rsp published spectrum reference --- RAh2000 Right Ascension J2000 (hours) h RAm2000 Right Ascension J2000 (minutes) min RAs2000 Right Ascension J2000 (seconds) s DE-2000 Declination J2000 (sign) --- DEd2000 Declination J2000 (degrees) deg DEm2000 Declination J2000 (minutes) arcmin DEs2000 Declination J2000 (seconds) arcsec Reference list with codes RefNum Reference number (rFlux, rPos, r_z) --- BibCode Bibliographic code, or CDS catalogue number --- Text of Reference --- Francois Ochsenbein CDS 1996 Dec 23 It is a pleasure to thank Michael Drinkwater <mjd@aaocbn.aao.gov.au> who supplied the tables in November 1996. VIII_34.xml Radio Sources Observed with the Culgoora Circular Array (CCA) at 80 and 160 MHz 8035 VIII/35 Radio Sources observed with Culgoora Circular Array Radio Sources Observed with the Culgoora Circular Array (CCA) at 80 and 160 MHz O B Slee Australian J. Phys. 48 143-186 1995 1995AuJPh..48..143S Radio sources This is a final, updated and recalibrated list of sources that were observed with the Culgoora Circular Array (CCA) in the interval 1970-1984. The list contains all the sources that were published in the Culgoora-1,2,3 Lists plus additional sources resulting from a survey of 353 Abell clusters of galaxies. The observations were made at 80 MHz and 160 MHz with HPBW in RA of 3.70' and 1.85' respectively. The beamwidth in Dec is wider by sec(30.3 + Dec). This list brings together all CCA measurements of flux density, position, spectral index and angular size, with limiting flux densities of 4 Jy at 80 MHz and 2 Jy at 160 MHz. References to the original Culgoora publications are given for each source. The sources were selected for CCA observations from the Parkes, 4C and Ohio catalogues if an extrapolation of the then existing spectral data indicated that the 80 MHz flux density would be > 5 Jy. In addition, about 300 additional sources were added from lists of special classes of objects such as those discovered at higher frequencies from surveys of the galactic plane, lists of pulsars and supernova remnants, from a list of nearby bright galaxies and finally from a CCA survey of 353 Abell clusters of galaxies. An area of 16'x16' was surveyed about the centres of 3500 fields, resulting in a total survey area of about 0.1 sr at 80 MHz. Nomenclature Notes: Sources from this catalogue are designated "Cul HHMM+DDd" in the literature. Note that the original Cul 1,2,3 lists have only HHMM+DD as a name, but the present names should be preferred.
The CCA survey Cul Source name number=1 the Cul designation contains the B1950 name of the source, using IAU recommended standards. The first four characters are the hours and minutes of right ascension, and the last four the signed declination in tenths of a degree (truncated). The source names in the original Culgoora-1,2,3 Lists contained the signed declination in degrees (truncated). IAU names given to tenths of declination in previous papers (e.g. ref #4 in section 9 below) may differ by one or two in the last digit. The Cul designation is followed by symbols: * An asterisk (*) following the source name denotes that this is the centroid of two or more components, which can be located in the maps and tables of references 3,4 and 5 below. The components are not always parts of the same source. # the flag '#' indicates that the Culgoora position was lost, but the source can confidently be identified with a source whose coordinates are given in the publication listed in the reference column. --- n_Cul Note on Source number=1 the Cul designation contains the B1950 name of the source, using IAU recommended standards. The first four characters are the hours and minutes of right ascension, and the last four the signed declination in tenths of a degree (truncated). The source names in the original Culgoora-1,2,3 Lists contained the signed declination in degrees (truncated). IAU names given to tenths of declination in previous papers (e.g. ref #4 in section 9 below) may differ by one or two in the last digit. The Cul designation is followed by symbols: * An asterisk (*) following the source name denotes that this is the centroid of two or more components, which can be located in the maps and tables of references 3,4 and 5 below. The components are not always parts of the same source. # the flag '#' indicates that the Culgoora position was lost, but the source can confidently be identified with a source whose coordinates are given in the publication listed in the reference column. --- o_S(160) Number of observations at 160 MHz number=2 These columns contain the numbers of independent observations at 160 MHz and 80 MHz respectively. Each observation consists of averaging 10-20 drift scans with the central 8 or 16 beams (spaced in declination) of the CCA. --- o_S(80) Number of observations at 80 MHz number=2 These columns contain the numbers of independent observations at 160 MHz and 80 MHz respectively. Each observation consists of averaging 10-20 drift scans with the central 8 or 16 beams (spaced in declination) of the CCA. --- RAh Right Ascension B1950 (hours) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. h RAm Right Ascension B1950 (minutes) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. min RAs Right Ascension B1950 (seconds) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. s DE- Declination B1950 (sign) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. --- DEd Declination B1950 (degrees) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. deg DEm Declination B1950 (minutes) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. arcmin DEs Declination B1950 (seconds) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. arcsec GLON Galactic longitude deg GLAT Galactic latitude deg l_S(160) Limit flag on S(160). --- S(160) Flux density at 160 MHz number=4 a recalibration of the flux scales was carried out by Slee & Siegman (1988MNRAS.235.1313S). This resulted in our increasing the flux density by an average of 10% at 80 MHz and 12% at 160 MHz. The 160 MHz flux densities of sources with contour maps (entries in the angular size columns) were obtained by integrating the brightness contours. Jy l_S(80) Limit flag on S(80). --- S(80) Flux density at 80 MHz number=4 a recalibration of the flux scales was carried out by Slee & Siegman (1988MNRAS.235.1313S). This resulted in our increasing the flux density by an average of 10% at 80 MHz and 12% at 160 MHz. The 160 MHz flux densities of sources with contour maps (entries in the angular size columns) were obtained by integrating the brightness contours. --- SpIndex Spectral index between 80 and 160 MHz number=5 this column contains the power-law spectral index between 80 and 160 MHz (S(nu) {prop.to} nu^SpIndex^). A negative spectral index implies that flux density is decreasing with frequency. --- l_MajAxis Limit flag on MajAxis --- MajAxis Major axis to 0.10 brightness at 160 MHz number=6 These columns contain the major and minor axes of a 2-dimensional Gaussian ellipse that has been fitted to the 160 MHz contour map together with the position angle of the major axis (from north through east).The axes are given to the 0.10 brightness points (1.82 x half-brightness diameter). Where only the major axis is presented as a lower limit of 1.8 arcmin, the limit was derived (at the 95% confidence level) from one-dimensional Gaussian fits to the drift profiles in RA and Dec. arcmin l_MinAxis Limit flag on MinAxis --- MinAxis Minor axis to 0.10 brightness at 160 MHz number=6 These columns contain the major and minor axes of a 2-dimensional Gaussian ellipse that has been fitted to the 160 MHz contour map together with the position angle of the major axis (from north through east).The axes are given to the 0.10 brightness points (1.82 x half-brightness diameter). Where only the major axis is presented as a lower limit of 1.8 arcmin, the limit was derived (at the 95% confidence level) from one-dimensional Gaussian fits to the drift profiles in RA and Dec. arcmin PA Position angle of major axis (east from north) number=6 These columns contain the major and minor axes of a 2-dimensional Gaussian ellipse that has been fitted to the 160 MHz contour map together with the position angle of the major axis (from north through east).The axes are given to the 0.10 brightness points (1.82 x half-brightness diameter). Where only the major axis is presented as a lower limit of 1.8 arcmin, the limit was derived (at the 95% confidence level) from one-dimensional Gaussian fits to the drift profiles in RA and Dec. deg Refs References number=7 References are 1 =1973AuJPS..27....1S Slee & Higgins 1973 (Culgoora-1 List) 2 =1975AuJPS..36....1S Slee & Higgins 1975 (Culgoora-2 List) 3 =1977AuJPS..43....1S Slee 1977 (Culgoora-3 List) 4 =1983PASAu...5..114S Slee & Siegman, Proc. ASA (Cluster Survey) 5 =1982PASAu...4..278S Slee, Siegman, & Mulhal (Culgoora-3 Analysis) 6 =1979PASAu...3..332S Slee & Quinn, Proc. ASA (Cluster Survey) 7 =1972ApL....12...75S Slee, Astrophys. Lett. (Bright Galaxies at 80 MHz) 8 =1972AuJPh..25..429D Dulk & Slee, Austral. (Supernova Remnants) 9 =1975PASAu...2....1S Slee & Sheridan, Proc.ASA (Cen-A & Pictor-A) 10 =1974Natur.248...33D Dulk & Slee (Sgr-A at 160 MHz) 11 =1991ApJS...75....1B Becker, White & Edwards (0736+016,2330+091,2349+135) 12 =1992ApJS...80..501O Owen, White & Burns (1005+007) 13 =1980BAAS...19.1048D Douglas (Texas Survey) Additional data in these papers include 80 MHz positions, optical identifications and beam broadening from the one-dimensional Gaussian fitting. The Culgoora-1,2,3 papers also contain tables listing the expected errors in flux density and position. References 3 and 4 contain the 160 MHz contour maps for many sources. Reference numbers 11,12,13 do not refer to Culgoora publications, but refer to papers containing sources that can be confidently identified with five sources, whose Culgoora positions have been lost. --- Heinz J. Andernach ESA-IUE 1996 Feb 19 Author's address: O.B Slee, Australia Telescope National Facility, CSIRO, Sydney <bslee@atnf.csiro.au> UNKNOWN UNKNOWN The basic table was formed by electronically scanning the Culgoora-3 list. Each line was later checked by visual comparison with the unscanned list and scanning errors were corrected manually. Additional sources were added manually from other references in <cul_ref>. Angular size information was extracted from references 4 and 5 and added manually to the final table. Positions of five sources for which Culgoora positions had been lost were identified with the help of the EINLINE service (telnet to einline.harvard.edu, login as 'einline' with no password) and H. Andernach (file r132.new). Note that the electronic version differs from the one published in AuJPh.48.143 in that it includes several dozen more upper limits at 160 MHz, taken from the listed references. VIII_35.xml A catalogue of 3235 radio sources at 408 MHz. 8036 VIII/36 The Second Bologna Survey A catalogue of 3235 radio sources at 408 MHz. G Colla C Fanti R Fanti A Ficarra L Formiggini E Gandolfi G Grueff C Lari L Padrielli G Roffi P Tomasi M Vigotti Astron. Astrophys. Suppl. Ser. 1 281 1970 1970A&AS....1..281C A catalogue of 3235 radio sources at 408 MHz. G Colla C Fanti R Fanti A Ficarra L Formiggini E Gandolfi C Lari B Marano L Padrielli P Tomasi Astron. Astrophys. Suppl. Ser. 7 1 1972 1972A&AS....7....1C A catalogue of 3235 radio sources at 408 MHz. G Colla C Fanti R Fanti A Ficarra L Formiggini E Gandolfi I Gioia C Lari B Marano L Padrielli P Tomasi Astron. Astrophys. Suppl. Ser. 11 291 1973 1973A&AS...11..291C A catalogue of 3235 radio sources at 408 MHz. C Fanti R Fanti A Ficarra L Padrielli Astron. Astrophys. Suppl. Ser. 18 147 1974 1974A&AS...18..147F VIII/37 : The Third Bologna Survey (B3) (Ficarra+ 1985) Radio sources Surveys This catalogue lists 9929 radio sources observed at 408MHz with the Bologna Northern Cross telescope.
B2 catalogue Name Full source name The full name always starts by B2, followed by the part number 1 to 4, and truncated 1950 position, eventually followed by a letter A,B,C... to have unique names. --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin Flux Peak flux at 408MHz the printed value was limited to two decimal figures. Jy Rem Remark (3C or 4C sources) --- Patricia Bauer CDS 1997 Sep 16 The file was kindly provided in September 1995 by Marzia Cannizzaro <CANNIZZARO@astbo1.bo.cnr.it> VIII_36.xml Third Bologna Survey at 408 MHz 8037 VIII/37 The Third Bologna Survey Third Bologna Survey at 408 MHz A Ficarra G Grueff G Tomassetti Astron. Astrophys. Suppl. Ser. 59 255 1985 1985A&AS...59..255F VIII/36 : The Second Bologna Servey (B2) Radio sources Surveys radio telescope radio sources catalogs This catalogue contains the first section of a sky survey performed at 408MHz with the 'Northern Cross' Radiotelescope. It contains about 13.000 radiosources. Although sources down to about 70mJy were measured, only sources brighter than 0.10Jy are retained in the catalogue. According to our estimate of confusion errors, this corresponds to a detection threshold of about 5{sigma}. The list is meant to include all the sources with a measured flux S>0.10Jy, in the sky area included between the declinations +37{deg}15' and +47{deg}37', epoch 1978.0. A number of zones however are affected by interferences, malfunctions, etc. The principal one is centered about the radiosource Cyg A, which is itself in the map, but not in the catalogue. The zone between RA 19h30m to 20h30m is entirely lacking, due to strong confusion. In the zone from 19h00m to 19h30m and from 20h30m to 21h00m, only sources brighter than 0.75Jy are listed, and to this level the catalogue is espected to be complete. For detailed discussion of the completeness of the catalogue see the original publication cited above.
The Bologna Third Catalogue B3 Source name, (IAU-style), eventually followed by a multiplicity letter A, B... --- RAh Right Ascension (1950.0) h RAm Right Ascension (1950.0) min RAs Right Ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Flux The source total flux. In the large majority of cases, this is practically equivalent to the peak flux Jy Fit Goodness of the fitting algorithm, related to the R.M.S. value of te residuals in the fitting matrix --- ACOD1 Four digit string indicating source reliability number=1 An algorithm was devised by which every source was marked with a four-digit number n1, n2, n3, n4 with each digit indicating a separate reason for problems, as follows: n1: a disturbing, strong source is present, very close in R.A., or very close in DEC. The flux ratio R is indicated by n1 and is n1 = R/10, truncated to the integer. n2: if non-zero, it indicates that the source lies in the vertical part of the cross-shaped area, and in the position of a grating response in N-S. It thus indicates a larger chance for the source to be spurious. The value itself is the rank of the grating response (n2 = 5 means the grating closer to the source, etc. down to n2 = 1) n3: if non-zero it means that the source is very close to a very strong source, although not in the cross-shaped area mentioned above. A circular area is defined with radius r=2.8sqrt(R)pix; n3 indicates how close the source is to the disturbing source, in units of 1/r n4: if n4 > 4, it indicates that the source lies within a disturbed area with the following code: 5: solar interferences 6: sidelobes of Cyg A 7: supernova remnant G160.4+2.8 (Felli et al., 1977A&AS...27..181F) 8: supernova remnant G166.0+4.3 (Willis, 1973A&A....26..237W) 9: man-made interferences If n4 < 4, it indicates that n4 (and no more) disturbing sources are present. In this case the previous digit refer to the stronger disturbing source. --- n_Diam If not blank the source were measured by a double source algorithm. R => resolved D => double --- Diam If the source is double: the separation arcmin Patricia Bauer CDS 1997 Sep 16 The file and the basic documentation were kindly provided by Marzia Cannizzaro <CANNIZZARO@astbo1.bo.cnr.it> in September 1995. VIII_37.xml The Parkes-MIT-NRAO (PMN) Surveys: II. Source catalog for the Southern Survey 8038 VIII/38 The Parkes-MIT-NRAO 4.85GHz The Parkes-MIT-NRAO (PMN) Surveys: II. Source catalog for the Southern Survey A E Wright M R Griffith B F Burke R D Ekers Astrophys. J. Suppl. Ser. 91 111 1994 1994ApJS...91..111W The Parkes-MIT-NRAO (PMN) Surveys: II. Source catalog for the Southern Survey M R Griffith A E Wright B F Burke R D Ekers Astrophys. J. Suppl. Ser. 90 179 1994 1994ApJS...90..179G The Parkes-MIT-NRAO (PMN) Surveys: II. Source catalog for the Southern Survey M R Griffith A E Wright B F Burke R D Ekers Astrophys. J. Suppl. Ser. 97 347 1995 1995ApJS...97..347G The Parkes-MIT-NRAO (PMN) Surveys: II. Source catalog for the Southern Survey A E Wright M R Griffith A J Hunt E Troup B F Burke R D Ekers Astrophys. J. Suppl. Ser. 103 145 1996 1996ApJS..103..145W VIII/15 : Parkes Radio Sources Catalogue (PKSCAT90) (Wright+ 1990) VIII/16 : Molonglo Reference Catalogue of Radio Sources (Large+ 1991) VIII/40 : GB6 catalog of radio sources at 4.85GHz (Gregory+ 1996) =1991Obs...111...72L "Molonglo Reference Catalogue of Radio Sources" Large M.I., Cram L.E., Brugess A.M.. 1991, The Observatory, 111, 72 =1993AJ....105.1666G (Paper I) "The Parkes-MIT-NRAO (PMN) surveys. Part I: The 4850MHz Surveys and data reduction" Griffith M.R., Wright A.E., 1993, Astron. J. 105, 1666 =1994ApJS...91..111W (Paper 2) "The Parkes-MIT-NRAO (PMN) surveys. Part II. Source catalog for the Southern Survey" Wright A.E., Griffith M.R., Burke B.F., Ekers R.D., 1994, Astrophys. J. Suppl. Ser. 91, 111 =1994ApJS...90..179G (Paper 3) "The Parkes-MIT-NRAO (PMN) surveys. Part III. Source catalog for the Tropical Survey Griffith M.R., Wright A.E., Burke B.F., Ekers R.D., 1994 Astrophys. J. Suppl. Ser. 90, 179 =1993AJ....106.1095C (Paper 4) "The Parkes-MIT-NRAO (PMN) surveys. Part IV. Maps for the Southern Survey" Condon J.J., Griffith M.R., Wright A.E., 1993, Astron. J. 106, 1095 =1994AJ....107.2115T (Paper 5) "The Parkes-MIT-NRAO (PMN) surveys. Part V. Maps for the Tropical Survey" Tasker N.J., Condon J.J., Wright A.E., Griffith M.R., 1994, Astron. J. 107, 2115 =1995ApJS...97..347G (Paper 6) "The Parkes-MIT-NRAO (PMN) surveys. Part VI. Source Catalog for the Equatorial Survey Griffith M.R., Wright A.E., Burke B.F., Ekers R.D., 1995 Astrophys. J. Suppl. Ser. 97, 347 =1996AJ....in.pressT (Paper 7) "The Parkes-MIT-NRAO (PMN) surveys. Part VII. Maps for the Equatorial survey and Zenith survey Tasker N.J., Wright A.E.,, Griffith M.R., 1996, Astron. J. (in press) =1996ApJS..103..145W (Paper 8) "The Parkes-MIT-NRAO (PMN) surveys. Part VIII. Source catalog for the zenith survey Wright A.E., Griffith M.R., Hunt A.J., Troup E., Burke B.F., Ekers R.D., 1996, Astrophys. J. Suppl. Ser. 103, 145 Radio sources Surveys radio continuum: general surveys The PMN surveys were made using the Parkes 64-m radio telescope at a frequency of 4850 MHz with the NRAO multibeam receiver mounted at the prime focus (for a full description of the observations see Griffith & Wright, 1993, Paper I). The surveys had a spatial resolution (full width half-maximum: FWHM) of approximately 4'.2 and were made during 1990 June and November. The PMN surveys were divided into several zones. These zones are listed in the following table, together with approximate flux limits and survey areas. -------------------------------------------------------------- Zone Name DEC limits (degrees) Flux limits Area (sr) File -------------------------------------------------------------- SOUTHERN -87.5< dec <-37 20 to 50 mJy 2.50 pmns ZENITH -37 < dec <-29 72 mJy 0.67 pmnz TROPICAL -29 < dec < -9.5 42 mJy 2.01 pmnt EQUATORIAL -9.5< dec <+10.0 40 mJy 1.90 pmne --------------------------------------------------------------- a point source catalogue was compiled directly from each of the survey zones by using an optimum filter method, as described by Griffith & Wright in detail in Paper 1. In addition, a set of images was produced for each zone in a manner very similar to that used by Condon et al. for the northern survey <VIII/40> (See e.g. our Paper 4). These maps have an effective resolution (FWHM) of about 5 arcmin. For more details, refer to the publications listed below for the relevant zone. Copyright: The Australia Telescope National Facility asserts copyright to this material. However, permission is granted for publication and reproduction for scholarly, educational, and private non-commercial use. Inquiries for potential commercial uses should be addressed to: Dr A.E. Wright, Parkes Observatory, PO Box 276, Parkes NSW, 2870, Australia
Southern Survey (-87.5 to -37) Zenith Survey (-37 to -29) Tropical Survey (-29 to -9.5) Equatorial Survey ( -9.5 to +10.0) PMNJ PMN J2000-based source name The J2000-derived source name. The names in this list have been derived from their J2000 coordinates, in a manner similar to that used in the PKSCAT90 catalog (Wright & Otrupcek, 1990, see cat. <VIII/15>). The first three letters, "PMN", denote the Parkes-MIT-NRAO survey, and the fourth letter, "J", denotes that the equinox and equator is J2000. The rest of the name is derived from the hours and minutes of the right ascension and the degrees and minutes of the declination (both J2000). For a few objects, the name (but not the source) is duplicated: in such cases an "a" or "b" was appended to the name. --- RAh Right ascension, J2000 h RAm R.A. min RAs R.A. s DE- Sign declination --- DEd Declination, J2000 deg DEm Dec. arcmin DEs Dec. arcsec Flux 4850 MHz flux density, derived from Fixed-Width fit (see Paper 1) mJy e_Flux Estimated standard error in Flux The estimated standard error for Flux. A standard error >99 mJy is listed as 99 mJy because of space limitations: the accurate value can be obtained from equation (4) in the printed paper. mJy GFlux 4850 MHz flux density, derived from the General-Width fit (see Paper 1) The 4850 MHz flux density derived from the General-Width fit (see Paper 1). This was done for and is only meaningful for sources greater than about 100 mJy. mJy e_GFlux Estimated standard error in GFlux The estimated standard error for GFlux. A standard error >99 mJy is listed as 99 mJy because of space limitations: the accurate value can be obtained from equation 4 in the printed paper. mJy Wid1 Semi-major axis of fitted Gaussian The semi-major and semi-minor axises of the fitted Gaussian in beam widths. A value of 1.0 = 2.1 arcmin --- Wid2 Semi-minor axis of fitted Gaussian --- PA Position angle of Wid1, east of north deg SI Spectral index The spectral index (log(S(v))/log(v)), computed between the present PMN flux densities at 4850 MHz and the 2700 MHz flux density from PKSCAT90 (cat. <VIII/15>), for sources common to both databases. --- Dflag Observation session flag Session in which the source was observed: "J" indicates the June 1990 session "N" indicates the November 1990 session --- Xflag Extended source flag An "X" indicates that the source is probably extended. This information is only available for sources whose Fixed-Width fit fluxes, before the application of the flux bias corrections (see Paper 1), were stronger than 100 mJy. --- Gflag Galactic plane flag A "G" indicates that the source lies within 10 degrees of the Galactic plane. --- Zflag Zenith flag a "Z" indicates a source which was observed within 6 degrees of the Parkes telescope's zenith (latitude -33deg) and has a flux < 60 mJy. --- Sflag Solar contamination flag An "S" indicates that the source lies within 5 degrees of solar contamination from the telescope's sidelobes and the data listed may be of lower quality. --- Pflag PKSCAT90 flag A "P" indicates that this source lies within 2' of a source listed in the PKSCAT90 database <VIII/15> and is probably the same object. --- Mflag Molonglo 408 MHz catalog flag An "M" indicates that this source lies within 2' of a source listed in the Molonglo 408 MHz catalog (Large et al. <VIII/16>) and is probably the same object. --- Francois Ochsenbein CDS 1996 Oct 02 It is a pleasure to thank Alan E. Wright for his kind help during this visit to CDS in March 1996. Authors: Alan E Wright ATNF, Parkes Observatory PO Box 276, Parkes, NSW, 2870, Australia <awright@atnf.csiro.au> Mark R. Griffith Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA & Dept. of Astronomy FM-20, University of Washington, Seattle, WA 98195 USA <griffith@astro.washington.edu> R D Ekers ATNF Headquarters PO Box 76, Epping, NSW, 2121, Australia <rekers@atnf.csiro.au> B. F. Burke Department of Physics, Massachusetts Institute of Technology Cambridge, MA 02139, USA Andrew J Hunt ATNF, Parkes Observatory PO Box 276, Parkes, NSW, 2870, Australia <ahunt@atnf.csiro.au> Euan Troup ATNF, Parkes Observatory PO Box 276, Parkes, NSW, 2870, Australia <etroup@atnf.csiro.au> VIII_38.xml Composite CO Survey of the Milky Way 8039 VIII/39 Composite CO Survey of the Milky Way Composite CO Survey of the Milky Way T M Dame H Ungerechts R S Cohen E J De Geus I A Grenier J May D C Murphy L A Nyman P Thaddeus ApJ 322 706 1987 1987ApJ...322..706D Radio sources Surveys Carbon monoxide This survey consists of CO J = 1-0 (115 GHz) spectra for the entire Galactic plane. The latitude coverage varies with longitude and in some regions extends from -25 degrees to +25 degrees. The observations were made with the Columbia/GISS 1.2 m telescope in New York City, and a twin telescope on Cerro Tololo in Chile. The angular resolution of the survey is 30' (square), the velocity resolution is 1.3 km/s and the sensitivity ranges from about 0.1 K/chan to 0.35 K/chan. The survey is presented as 720 latitude-velocity maps in FITS format, one for each 30' of longitude from -180.0 deg to +179.5 deg, and one velocity-integrated map covering the entire plane. The velocity range of each file is -300 km/s to +300 km/s. The survey has been updated to include some additional data, more careful reprojections of the regions that were originally mapped in equatorial coordinates, and improved estimates of the absolute calibration of the CO intensities (Digel and Dame 1995, unpublished).
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longitude 177.5 deg vb_716.fit Latitude-velocity map for longitude 178.0 deg vb_717.fit Latitude-velocity map for longitude 178.5 deg vb_718.fit Latitude-velocity map for longitude 179.0 deg vb_719.fit Latitude-velocity map for longitude 179.5 deg Seth Digel SSDOO 1996 May 10 VIII_39.xml The GB6 catalog of radio sources 8040 VIII/40 GB6 catalog of radio sources The GB6 catalog of radio sources P C Gregory W K Scott K Douglas J J Condon Astrophys. J. Suppl. Ser. 103 427 1996 1996ApJS..103..427G VIII/14 : 87GB Catalog of radio sources (Gregory et al., 1991) VIII/38 : The PMN Surveys at 4.85GHz (Griffith+ 1993-1996) Radio sources catalogs radio continuum: galaxies surveys The final set of sky maps from the Green Bank 4.85 GHz survey (Condon J.J., Broderick J.J., Seielstad G.A., Douglas K., & Gregory P.C. in 1994AJ....107.1829C) was used to construct the GB6 Catalog of sources stronger than S ~ 18 mJy in the declination range 0deg < Dec. < +75deg (Gregory P.C., Scott W.K., Douglas K., & Condon J.J. in 1996ApJS..103..427G). There are two machine-readable versions of the GB6 catalog, with coordinates precessed to B1950 (file b1950.dat) and J2000 (file j2000.dat). Each catalog file contains one line per source (75,162 lines each), and the sources are sorted by increasing B1950 or J2000 right ascension. The Green Bank 4.85GHz (lambda~6cm) survey was made with the NRAO seven-beam receiver on the (former) 91m telescope during 1986 November and 1987 October. The final set of sky maps covering the declination band 0deg<Dec.<+75deg was constructed with data from both epochs. Its noise and position errors are nearly a factor of 2^(1/2)^ smaller than in the epoch 1987 maps, from which the 87GB catalog <VIII/14> of 54,579 sources stronger than S~25mJy was extracted. Therefore, we used the new maps to make the GB6 catalog of 75,162 discrete sources with angular sizes phi<=10.5arcmin and flux densities S>=18mJy. This catalog is available in machine-readable versions with either B1950 or J2000 positions and as a printed book with B1950 positions. The GB6 weighted differential source counts S^(5/2)n(S) between 18 mJy and 7Jy agree well with evolutionary models based on independent data.
GB6 catalog, B1950 coordinates GB6 catalog, J2000 coordinates RAh Right ascension h RAm Right ascension min RAs Right ascension s e_RAs Uncertainty in R.A. s DE- Sign of declination --- DEd Declination deg DEm Declination arcmin DEs Declination arcsec e_DEs Uncertainty in declination arcsec GLAT Galactic latitude deg GLON Galactic longitude deg Flux 4.85 GHz peak flux density mJy e_Flux Uncertainty in peak flux density mJy Bflag for sources near the border number=1 The GB6 catalog is the result of merging 288 catalogs, each of which came from a single GB6 image covering about 15X15deg of sky. Sources found near the border of an image are flagged 'B'. The borders of these images overlap, so duplication among sources which appeared in two or more catalogs had to be removed from the final GB6 catalog. Normally, the one fit without the 'B' flag was chosen. Thus there are two classes of 'B' sources which remain in the final catalog: (1) All sources near the upper (+75 deg) and lower (0 deg) declination limits of the images. (2) Sources elsewhere that are just at the catalog limit, so the fit was just above the limit near the border of one image and just below the limit in the overlapping image(s). --- Eflag for significant extension --- Wflag for warning (weak source with large Zero) --- Cflag for confusion (near a stronger source) --- MajAxis Normalized FWHM major axis / beam size --- MinAxis Normalized FWHM minor axis / beam size --- PA Fitted major axis position angle (degrees east of north) deg Zero Local sky level, Z / beam mJy Xmap Map pixel column number (from left) pix Ymap Map pixel row number (from bottom) pix CDS 1996 Sep 06 AAS CD-ROM series, Volume 6, 1996 UNKNOWN UNKNOWN If you would like to order the printed catalog or have any questions, comments, or special requests, please contact Jim Condon by e-mail at Internet address <jcondon@nrao.edu>. VIII_40.xml The UTR-2 Very Low-Frequency Sky Survey Data Decametric survey of discrete sources in the northern sky. II. Source catalogue in the range of declinations +10 to +20 8041 VIII/41 The UTR-2 Very Low-Frequency Sky Survey Data The UTR-2 Very Low-Frequency Sky Survey Data Decametric survey of discrete sources in the northern sky. II. Source catalogue in the range of declinations +10 to +20 S Ya Braude A V Megn S L Rashokovski B P Ryabov N K Sharykin K P Sokolov A P Tkatchenko I N Zhouk Astrophys. Space Sci. 54 37 1978 1978Ap&SS..54...37B The UTR-2 Very Low-Frequency Sky Survey Data Decametric survey of discrete sources in the northern sky. II. Source catalogue in the range of declinations +10 to +20 S Ya Braude A V Megn K P Sokolov A P Tkatchenko N K Sharykin Astrophys. Space Sci. 64 73 1979 1979Ap&SS..64...73B The UTR-2 Very Low-Frequency Sky Survey Data Decametric survey of discrete sources in the northern sky. II. Source catalogue in the range of declinations +10 to +20 S Ya Braude A P Miroshnitchenko K P Sokolov N K Sharykin Astrophys. Space Sci. 74 409 1981 1981Ap&SS..74..409B The UTR-2 Very Low-Frequency Sky Survey Data Decametric survey of discrete sources in the northern sky. II. Source catalogue in the range of declinations +10 to +20 S Ya Braude N K Sharykin K P Sokolov S M Zakcharenko Astrophys. Space Sci. 111 1 1985 1985Ap&SS.111....1B The UTR-2 Very Low-Frequency Sky Survey Data Decametric survey of discrete sources in the northern sky. II. Source catalogue in the range of declinations +10 to +20 S Ya Braude K P Sokolov S M Zakcharenko Astrophys. Space Sci. 213 1 1994 1994Ap&SS.213....1B Radio sources The results of the very-low frequency (16.7MHz) survey of discrete sources made with the UTR-2 radio telescope is presented. The survey concerns the declination zones -13{deg} to -2{deg}, 0{deg} to 20{deg}, and 41{deg} to 60{deg}. The UTR-2 radio source catalogue contains an estimate of the coordinates and flux densities of 1819 sources measured at a number of the lowest frequencies used in contemporary radio astronomy within the range from 10 to 25 MHz. The catalogue is made of two parts: mean.dat: the averaged values of the coordinates and the corresponding errors, the source flux-density at the middle UTR-2 frequency 16.7 MHz as obtained from measured spectrum of the source at all UTR-2 frequencies and its error, the value of measured low-frequency spectral index with respect to which the estimate of has been obtained, the parameter W characterizing the integral reliability of the obtained source estimates and the corresponding object name from higher-frequency radio survey provided the source has been identified. To indicate the integral readability of the source parameters obtained we used the symbols A, B and C. These reliability estimates take into account the total number of measurements, coordinate scatter, number of frequencies and hour-angle settings at which the source parameters have been evaluated. The highly reliable observation results have been marked with symbol A . The sources whose parameters can be used without an additional analysis are marked with B and sources whose parameters are to be used with care have been marked with C. data.dat: this file contains the experimental estimates of the source coordinates and flux densities as well as their errors at each operating frequency of the UTR-2 in the order of their increasing; the total number (N) of successive observations according to which the estimates were obtained and the number of different hour-angle settings (NRA) of the reception pattern at which the source was observed. In cases when the observations did not allow us to obtain a reliable estimates of a source flux density the catalogue contains only their upper limits which are not accompanied by errors. The approximated values of as well as low-frequency spectral indices are presented only for those sources which have flux density estimates obtained at not less than three different UTR-2 frequencies.
Averaged values and cross-identifications Name Source name (individual data in file data.dat) the name includes the publication number (2,5,7,9,11), "GRB" (the B indicates that 1950 positions are used in the name). hours and minutes of RA(1950), and degrees of Declination(1950). Up to 6 lines in file data.dat contain the experimental estimates of the source coordinates and flux densities as well as their errors at each operating frequency of the UTR-2. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s e_RAs rms uncertainty on RAs s DEdeg Declination (1950) deg e_DEdeg rms uncertainty on DEdeg deg Freq Frequency MHz l_S Limit flag on fLux density --- S Flux-density at frequency Freq Jy e_S rms uncertainty on flux density % SI Low-frequency spectral index --- e_SI rms uncertainty on SI --- W Integrated estimate of reliability the reliability index takes the values: A: Highly reliable data B: Results that can be used without an additional analysis C: Data requiring additional analysis, up to an examination of the original analogue records --- OtherName Other names --- Experimental estimates at each operating frequency of the UTR-2 Name Source name, as in file mean.dat the name includes the publication number (2,5,7,9,11), "GRB" (the B indicates that 1950 positions are used in the name). hours and minutes of RA(1950), and degrees of Declination(1950). Up to 6 lines in file data.dat contain the experimental estimates of the source coordinates and flux densities as well as their errors at each operating frequency of the UTR-2. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s e_RAs rms uncertainty on RAs s DEdeg Declination (1950) deg e_DEdeg rms uncertainty on DEdeg deg Freq Frequency MHz l_S Limit flag on fLux density --- S Flux-density at frequency Freq Jy e_S rms uncertainty on flux density % N Total number of successful measurements --- NRA Number of angular positions on RA of the reception pattern at which the source was observed --- K.P. Sokolov Ukrainia Francois Ochsenbein CDS 1997 Sep 15 For any information concerning to the UTR-2 Very Low-Frequency Sky Survey, please, contact to: Dr. K.P. Sokolov Institute of Rsdio Astronomy 4, Krasnoznamennaya Street Kharkov 310002 UKRAINE E-mail:rai@ira.kharkov.ua FAX: 38 (0572) 47-65-06 Phone: 38 (0572) 45-10-14 (office), 38 0572-44-09-37 (home) VIII_41.xml The Texas survey of radio sources covering -35.5{deg} < {delta} < 71.5{deg} at 365MHz 8042 VIII/42 Texas Survey of radio sources at 365MHz The Texas survey of radio sources covering -35.5{deg} < {delta} < 71.5{deg} at 365MHz J N Douglas F N Bash F A Bozyan G W Torrence C Wolfe Astron. J. 111 1945 1996 1996AJ....111.1945D Radio sources We present the Texas Survey of discrete radio sources between -35.5deg and 71.5deg declination (B1950), which was carried out at 365MHz with the Texas Interferometer during 1974-1983. The Survey lists accurate positions with internal errors of about an arcsecond, flux densities which for strong point sources have internal errors of about 1% and total errors of about 5%, simple structure models and indications of spectrum and variability for 66841 sources. Results of comparisons with other data are presented, and show that the Survey is 90% complete at 0.4Jy and 80% complete at 0.25Jy, is nearly free from spurious sources, and has a lobeshift incidence which is reasonably described by quality flags associated with each source.
The University of Texas Radio Astronomy Observatory (UTRAO) has carried out, with the Texas Interferometer, a 365MHz survey of the sky from -35.5 to +71.5{deg} declination, which was intended to be complete to a flux density level of 0.25Jy, to provide positions with an accuracy of about 1arcsec in both coordinates, to give accurate flux densities and indication of source variability, and to give rough structure models for each source. The observations began in 1974 and were completed in 1983. A preliminary version of one declination strip was published (Douglas et al., 1980), and a number of intermediate versions of the survey have been privately circulated for various purposes pending completion of the final analysis and adjustment of the data.
The Texas Survey Strip Main strip The catalog was originally decomposed in 10 tables table3a to table3j corresponding to the 10 declination strips: ----------------------- Strip Range of Decl. name ----------------------- A -26 [-357,-187] B -12 [-186,-064] C -01 [-063,+039] D +09 [+040,+135] E +18 [+136,+226] F +27 [+227,+316] G +36 [+317,+406] H +45 [+407,+499] I +55 [+500,+598] J +65 [+599,+715] --- Aflg * means simpler model(s) exist --- TXS Source name The TXS source name is constructed from the hours and minutes of right ascension, the sign of declination, and truncated tenths of degrees of declination: hhmmsddd. Because of a final position system adjustment, the source name may not agree with the position in the table, but should be used regardless. --- XPVRflg # of subbeams outside the PVR --- Mflg goodness of model fit --- Eflg influence of environment --- Lflg lobeshift probability --- LVflg # of low-visibility subbeams --- RAh Right Ascension 1950 h RAm Right Ascension 1950 min RAs Right Ascension 1950 s e_RAs Right Ascension error s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec e_DEs Declination error arcsec n_S365 X if flux <0.15 Jy --- S365 365 MHz flux density Jy e_S365 Internal rms flux error Jy SNflg signal-to-noise flag the Signal-to-Noise flag is set to: X when S/N < 4 Y when 4 <= S/N < 5 Z when 5 <= S/N < 7 blank when S/N >=7 --- Spec spectral index --- e_Spec [0,1[ error in spectral index --- Chi2 chi-squared flux residual, 2 dof values of Chi2 are statistically > 5.99 for 5% of non-variable sources > 9.21 for 1% of non-variable sources (Vstar set to '*') >13.82 for 0.1% of non-variable sources --- u_Chi2 X means value of Chi2 is suspect --- Vstar * means source may be variable --- Sep component separation in double model arcsec --- field separator --- e_Sep error in Sep arcsec --- field separator --- Struct Structure model type 'P ' = Point model 'D ' = Double model 'AD' = Asymmetric Double model ; the 'q' asymmetry parameter is then set. --- q Asymetry q parameter for AD model % --- field separator --- e_q 100xerror in asymmetry parameter q % --- field separator --- Xi position angle of double deg --- field separator --- e_Xi error in position angle deg --- field separator --- RAOflg RA overlap zone flag * means this is one of two versions of this catalog line, because the source was in an RA overlap zone; the RA zone is then given in the RAOZ column. --- DEOflg DE overlap zone flag * means this is one of two versions of this catalog line, because the source was observed separately in two observation declination strips; the DE zone is then given in the DEOZ column. --- --- field separator --- KA2 second most likely RA lobe --- --- field separator --- KD2 second most likely Dec lobe --- --- field separator --- RAOZ RA overlap zone --- DEOZ Dec overlap zone --- strp Observation strip source line taken from observation strip and segment from which the catalog line was obtained. For example, in TXS 0000+178, strp=181 means that the catalog line came from the +18{deg} observation strip, RA segment 1. Some sources came from Version 6 of the Texas Survey ('TS6' in strp field) or Version 7 ('TS7' in strp field) --- The sources in the simpler model. Strip Main strip, as in txs.dat file. --- TXS Source name The name is that of the corresponding Survey source line in file txs.dat --- XPVRflg # of subbeams outside the PVR --- Mflg goodness of model fit --- Eflg influence of environment --- Lflg lobeshift probability --- LVflg # of low-visibility subbeams --- RAh Right Ascension 1950 h RAm Right Ascension 1950 min RAs Right Ascension 1950 s e_RAs Right Ascension error s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec e_DEs Declination error arcsec n_S365 X if flux <0.15 Jy --- S365 365 MHz flux density Jy e_S365 Internal rms flux error Jy SNflg signal-to-noise flag --- Spec spectral index --- e_Spec [0,1[ error in spectral index --- Sep component separation in double model arcsec Struct structure model type Point model is 'P'; Double model is 'D'; there are no AD models in the "Simpler models". --- Xi position angle of double deg RAOZ RA overlap zone --- DEOZ Dec overlap zone --- strp Observation strip source line taken from --- Francois Ochsenbein CDS 1996 Oct 23 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 6, 1996. * At CDS, October 1996: The original 'table3*' tables were merged into the "txs.dat" file, and 'table4*' tables into the "simpler.dat" file, but the table number was inserted in byte one. VIII_42.xml A radio survey of clusters of galaxies I. 11.1 cm observations of A 591, A 754, A 1066, A 1314, A 1517, A 2094, A 2142, A 2255, A 2256, A 2319 and A 2462. 8043 VIII/43 Radio survey of clusters of galaxies A radio survey of clusters of galaxies I. 11.1 cm observations of A 591, A 754, A 1066, A 1314, A 1517, A 2094, A 2142, A 2255, A 2256, A 2319 and A 2462. C G T Haslam P P Kronberg H Waldthausen R Wielebinski D Schallwich Astron. Astrophys., Suppl. Ser. 31 99 1978 1978A&AS...31...99H A radio survey of clusters of galaxies I. 11.1 cm observations of A 591, A 754, A 1066, A 1314, A 1517, A 2094, A 2142, A 2255, A 2256, A 2319 and A 2462. H Waldthausen C G T Haslam R Wielebinski P P Kronberg Astron. Astrophys., Suppl. Ser. 36 237 1979 1979A&AS...36..237W A radio survey of clusters of galaxies I. 11.1 cm observations of A 591, A 754, A 1066, A 1314, A 1517, A 2094, A 2142, A 2255, A 2256, A 2319 and A 2462. H Andernach H Waldthausen R Wielebinski Astron. Astrophys., Suppl. Ser. 41 339 1980 1980A&AS...41..339A A radio survey of clusters of galaxies I. 11.1 cm observations of A 591, A 754, A 1066, A 1314, A 1517, A 2094, A 2142, A 2255, A 2256, A 2319 and A 2462. H Andernach D Schallwich C G T Haslam R Wielebinski Astron. Astrophys., Suppl. Ser. 43 155 1981 1981A&AS...43..155A A radio survey of clusters of galaxies I. 11.1 cm observations of A 591, A 754, A 1066, A 1314, A 1517, A 2094, A 2142, A 2255, A 2256, A 2319 and A 2462. H Andernach A Sievers A Kus J Schnaubelt Astron. Astrophys., Suppl. Ser. 65 561 1986 1986A&AS...65..561A A radio survey of clusters of galaxies I. 11.1 cm observations of A 591, A 754, A 1066, A 1314, A 1517, A 2094, A 2142, A 2255, A 2256, A 2319 and A 2462. H Andernach T Han A Sievers H -P Reuter N Junkes R Wielebinski Astron. Astrophys., Suppl. Ser. 73 265 1988 1988A&AS...73..265A A radio survey of clusters of galaxies I. 11.1 cm observations of A 591, A 754, A 1066, A 1314, A 1517, A 2094, A 2142, A 2255, A 2256, A 2319 and A 2462. H -P Reuter H Andernach Astron. Astrophys., Suppl. Ser. 82 279 1990 1990A&AS...82..279R Clusters, galaxy Radio sources Spectroscopy Redshifts References Morphology galaxies: clusters: general continuum maps spectral index radio spectra linear polarization radio sources spectra of radio sources optical and IR identification of radio sources Observations of Abell clusters at 11.1, 6.2, 6.3 and 2.8cm with the 100m Effelsberg telescope. The data were compiled by H.J. Andernach.
Optical data for the clusters studied (Paper 3) Abell Abell cluster number --- RAh Right ascension (1950) h RAm Right ascension (1950) min DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin BM Bautz-Morgan class --- n_BM Note on BM number=1 * : Corwin's estimate (1974AJ.....79.1356C) --- RS Rood-Sastry classification --- n_RS Note on RS number=2 + = estimate by Bahcall, Harris and Strom (1976ApJ...209L..17B) * = Owen's (1975AJ.....80..263O) estimate : = uncertainty flag --- Rich Richness class (Abell, 1958 Cat. <VII/4>) --- Dist Distance (Abell, 1958 Cat. <VII/4>) Mpc zEst Estimated Redshift --- n_zEst Note on zEst number=3 Ow: Owen (1974AJ.....79..427O) *: Owen (1975AJ.....80..263O) R: Riley (1975MNRAS.170...53R) MH: Mills & Hoskins (1977AuJPh..30..509M) N: Noonan (1973AJ.....78...26N) S: Sargent (1973PASP...85..281S) B: Bridle and Folamont (1976A&A....52..107B) C: Corwin (1974AJ.....79.1356C) --- zMeas Measured redshift --- n_zMeas Note on zMeas number=3 Ow: Owen (1974AJ.....79..427O) *: Owen (1975AJ.....80..263O) R: Riley (1975MNRAS.170...53R) MH: Mills & Hoskins (1977AuJPh..30..509M) N: Noonan (1973AJ.....78...26N) S: Sargent (1973PASP...85..281S) B: Bridle and Folamont (1976A&A....52..107B) C: Corwin (1974AJ.....79.1356C) --- RAbell Abell radius arcmin RCluster Cluster radius number=4 Estimates from Leir & Van den Bergth (1977ApJS...34..381L) arcmin magBr Brightest galaxy magnitude mag mag10th 10th brightest galaxy magnitude mag aMaj Major axis of the brightest galaxy arcmin aMin Minor axis of the brightest galaxy arcmin DistC Distance from center arcmin Xname Possible identification with an X-ray source number=5 Giaconni et al. (1974ApJS...27...37G) Cooke et al., (1978MNRAS.182..489C) Forman et al., (1978ApJS...38..357F) For A 2079, 3U 1526+29 not fulfilling the 3U catalogue criteria --- l_RadX Limit flag on RadX --- RadX X-ray core radius arcmin e_RadX rms uncertainty on RadX arcmin RadO Optical core radius arcmin Optical and X-ray data for the clusters studied (Papers 3 and 4) Abell Abell cluster number --- RAh Right ascension (1950) h RAm Right ascension (1950) min NotePos Note on position --- DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin BM Bautz-Morgan class --- r_BM BM references (see ref4 file) number=1 a: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), Leir and van den Bergh (1977ApJS...34..381L), and Mills and Hoskins (1977AuJPh..30..867M). b: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), and Mills and Hoskins (1977uJPh..30..867M). c: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), and Leir and van den Bergh (1977ApJS...34..381L) d: mean of estimates by Owen (1975ApJ...195..593O), Leir and van den Bergh, (977ApJS...34..381L) and Mills and Hoskins (1977AuJPh..30..867M). e: Both A2255 and A2319 may consist of two clusters nearly superimposed along the line of sight, but only for A2319 we use the weighted mean of the redshifts of the subclusters. f: Bahcall (1975ApJ...198..249B) found the cluster centre to be coincident with the dominant cD galaxy. We measured the position of this galaxy on our overlay and took that as the cluster centre position. g: Measured redshift for foreground (?) galaxy z=0.036C h: The radiosource in A1836 is identified with a foreground galaxy with z=0.025C --- RS Rood-Sastry classification --- r_RS Reference on RS (see ref4 file) --- Rich Richness class (Abell, 1958 Cat. <VII/4>) --- Dist Distance (Abell, 1958 Cat. <VII/4>) Mpc z Redshift --- n_z Note on Redshift number=1 a: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), Leir and van den Bergh (1977ApJS...34..381L), and Mills and Hoskins (1977AuJPh..30..867M). b: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), and Mills and Hoskins (1977uJPh..30..867M). c: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), and Leir and van den Bergh (1977ApJS...34..381L) d: mean of estimates by Owen (1975ApJ...195..593O), Leir and van den Bergh, (977ApJS...34..381L) and Mills and Hoskins (1977AuJPh..30..867M). e: Both A2255 and A2319 may consist of two clusters nearly superimposed along the line of sight, but only for A2319 we use the weighted mean of the redshifts of the subclusters. f: Bahcall (1975ApJ...198..249B) found the cluster centre to be coincident with the dominant cD galaxy. We measured the position of this galaxy on our overlay and took that as the cluster centre position. g: Measured redshift for foreground (?) galaxy z=0.036C h: The radiosource in A1836 is identified with a foreground galaxy with z=0.025C --- r_z Redshift reference (see ref4 file) --- n_r_z Note on redshift reference number=1 a: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), Leir and van den Bergh (1977ApJS...34..381L), and Mills and Hoskins (1977AuJPh..30..867M). b: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), and Mills and Hoskins (1977uJPh..30..867M). c: mean of estimates by Corwin (1974AJ.....79.1356C), Owen (1975ApJ...195..593O), and Leir and van den Bergh (1977ApJS...34..381L) d: mean of estimates by Owen (1975ApJ...195..593O), Leir and van den Bergh, (977ApJS...34..381L) and Mills and Hoskins (1977AuJPh..30..867M). e: Both A2255 and A2319 may consist of two clusters nearly superimposed along the line of sight, but only for A2319 we use the weighted mean of the redshifts of the subclusters. f: Bahcall (1975ApJ...198..249B) found the cluster centre to be coincident with the dominant cD galaxy. We measured the position of this galaxy on our overlay and took that as the cluster centre position. g: Measured redshift for foreground (?) galaxy z=0.036C h: The radiosource in A1836 is identified with a foreground galaxy with z=0.025C --- Ngal Number of galaxies used for determining the redshift number=5 A blank implies that the number was not given by the author or the redshift is an estimate only. ---- RAbell Abell radius arcmin RCluster Cluster radius number=2 Data from Leir and van den Bergh (1977ApJS...34..381L) arcmin magBr Brightest galaxy magnitude number=2 Data from Leir and van den Bergh (1977ApJS...34..381L) mag mag10th 10th brightest galaxy magnitude number=3 When only the 10th magnitude is given, the entry is from Sastry and Rood (1971ApJS...83..371S) mag aMaj Major axis of the brightest galaxy number=2 Data from Leir and van den Bergh (1977ApJS...34..381L) mm aMin Minor axis of the brightest galaxy number=2 Data from Leir and van den Bergh (1977ApJS...34..381L) mm Map I,II : states whether 11.1cm data were already published in Paper I or II X : Refers to 6.2cm Effelsberg observations presented in Paper III --- Xnames X-ray sources associated with the cluster number=4 Detection of an X-ray source in the 3U/4U or 2A catalogues (Giaconni et al., 1974ApJS...27...37G; Forman et al. 1978ApJS...38..357F; Cooke et al. 1978MNRAS.182..489C) or with the HEAO-A (HA) or HEAO-B (HB) satellites (Schwartz et al., 1979ApJ...231L.105S; Ku, 1979, Priv. communication; upper limits (in brackets): Ulmer et al., 1980ApJ...235..351U) For A2079, 3U 1526+29 not fulfilling the 3U criteria --- RefX References for X-ray flux (see ref4 file) --- RefXsp References for X-ray spectra (see ref4 file) --- l_RadX Limit flag on X-ray core radius --- RadX X-ray core radius arcmin r_RadX X-ray core radius reference (see ref4 file) --- RadO Optical core radius arcmin Relevant Parameters for observed Cluster (Papers 6 and Paper 7) Abell Abell cluster number --- m_Abell Multiplicity index on Abell number --- RAh Optical right ascension (1950) h RAm Optical right ascension (1950) min RAs Optical right ascension (1950) s DE- Declination sign --- DEd Optical declination (1950) deg DEm Optical declination (1950) arcmin DEs Optical declination (1950) arcsec RefPos Position reference number=1 References are in ref5 file --- RS Rood-Sastry classification --- r_RS References for RS classification number=1 References are in ref5 file --- BM Bautz-Morgan classification --- u_BM Uncertainty flag on BM classification --- r_BM References for BM classification number=1 References are in ref5 file --- Dist Distance (Abell 1958, Cat. <VII/4>) Mpc Rich Richness (Abell 1958, Cat. <VII/4>) --- z Redshift --- n_z e = estimated number=2 a: recently z=0.0318 (RAbell=56.7') had been measured (Kalinkov 1985, priv. comm.) b: a more recent estimate is z=0.0856, RAbell=22.8' (Kalinkov 1985, priv. comm.) --- r_z Redshift reference number=1 References are in ref5 file --- RAbell Apparent Abell radius arcmin n_RAbell Note on Abell radius number=2 a: recently z=0.0318 (RAbell=56.7') had been measured (Kalinkov 1985, priv. comm.) b: a more recent estimate is z=0.0856, RAbell=22.8' (Kalinkov 1985, priv. comm.) --- ROpt Optical radius arcmin u_ROpt Uncertainty flag on ROpt --- l_log(LX) Limit flag on log(LX) --- log(LX) X-ray cluster luminosity 10-7W r_log(LX) X-ray cluster luminosity reference number=1 References are in ref5 file --- Obs11.1cm Observation Epoch minus 1900.0 at 11.1cm --- Obs6.3cm Observation Epoch minus 1900.0 at 6.3cm --- Obs2.8cm Observation Epoch minus 1900.0 at 2.8cm --- Optical and radio identifications of IRAS point sources (Paper 7) Abell Abell cluster name --- m_Abell Multiplicity (several clusters) --- RAh Infrared right ascension (B1950) h RAm Infrared right ascension (B1950) min RAs Infrared right ascension (B1950) s DE- Declination sign --- DEd Infrared declination (B1950) deg DEm Infrared declination (B1950) arcmin DEs Infrared declination (B1950) arcsec l_S100/S60 Limit flag on S100/S60 --- S100/S60 Ratio of IR flux densities (S100um/S60um) --- l_SpI Limit flag on SpI --- SpI Radio-IR spectral index (between 2.7GHz and 100um) --- IdOpt Optical identification --- Rem Remarks --- 11.1cm (2.7GHz) radio data (Papers 1 and 2) Source Source name number=1 We have labelled each prominent source with a subnumber (A85.1 etc.), regardless of cluster membership, in increasing order of right ascension for each cluster area mapped. We have only labelled the most prominent sources. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec u_Pos Uncertainty flag on position --- l_S2.7GHz Limit flag on S2.7GHz --- S2.7GHz Flux density at 2695 MHz (11.1cm) mJy u_S2.7GHz Uncertainty flag on S2.7GHz --- Catal Source catalogue name --- Ref References (see ref1 file) --- 11.1cm (2.7GHz) radio data, and optical identifications (Papers 4, 5, 6, and 7) Source Source name --- n_Source Note on Source number=1 A: Source reported by Swarup (1984JApA....5..139S) B: central part only C: position from Harris et al. (1980A&AS...39..215H) D: For A1060 and A2199 (data of 1988A&AS...73..265A), a renumbering was necessary for some sources. E: Renumbered with respect to data in 1980A&AS...41..339A F: A1060.0 same as A1060.1 in 1980A&AS...41..339A (r4750 file) a: source claimed by Slee & Quinn 1980PASAu...3..332S b: position from Andernach et al. 1980A&AS...41..339A (paper III) d: source claimed by Owen 1974AJ.....79..427O g: source named A2220.1 in Andernach et al. 1980A&AS...41..339A (paper III) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec NotePos Note on position number=2 A: source detected by Mayer (1980, Ph.D. Thesis, Cambridge University B: 11 cm position a: from McHardy (1978MNRAS.184..783M) b: position from Andernach et al. 1980A&AS...41..339A (paper III) %c: from Dickey and Salpeter (1984ApJ...284..461D) d: from Dickey and Salpeter (1984ApJ...284..461D) and uncertain value e: from Perola and Valentijn (1979A&A....73...54P) f: east part of map is less sensitive i: correction of typo in original paper j: position from McHardy (1978MNRAS.185..927M l: same as A1060.1 of Paper III (1980A&AS...41..339A) m: central part of map is more sensitive n: position from Lauberts (1982, Cat. <VII/34>) o: detected by Fanti et al. (1983A&AS...51..179F, 1983A&AS...52..411F) p: detected by Douglas et al. (1973AJ.....78....1D) q: B2 position (Colla et al., 1972A&AS....7....1C) s: NE component of 4CP66.16.1 u: data for outer part v: data for central part ':' : uncertainty flag --- l_S2.7GHz Limit flag on S2.7GHz --- S2.7GHz Integrated flux density at 2.7GHz mJy u_S2.7GHz Uncertainty flag on S2.7GHz --- e_S2.7GHz rms uncertainty on S2.7GHz mJy n_S2.7GHz Note number=3 4: see table4e for Flux density to Xi data 5: see table5e for Flux density to Xi data E: including two components 8' SE and NW of main source H: distorted due to map artefact a: includes N extension b: including overall extent c: including extension due SW d: not including extensions due NE and SE e: assuming a point source at the given position g: excluding extension due E h: Three satellite sources provide for another 50 mJy i: not including extension due W k: including overall extent t: not including the SE extension --- rmsI rms noise level at 2.7GHz in total intensity (in mJy/beam area) mJy rmsP rms noise level at 2.7GHz in polarized intensity (in mJy/beam area) mJy n_rmsI Note on rmsI and rmsP number=2 A: source detected by Mayer (1980, Ph.D. Thesis, Cambridge University B: 11 cm position a: from McHardy (1978MNRAS.184..783M) b: position from Andernach et al. 1980A&AS...41..339A (paper III) %c: from Dickey and Salpeter (1984ApJ...284..461D) d: from Dickey and Salpeter (1984ApJ...284..461D) and uncertain value e: from Perola and Valentijn (1979A&A....73...54P) f: east part of map is less sensitive i: correction of typo in original paper j: position from McHardy (1978MNRAS.185..927M l: same as A1060.1 of Paper III (1980A&AS...41..339A) m: central part of map is more sensitive n: position from Lauberts (1982, Cat. <VII/34>) o: detected by Fanti et al. (1983A&AS...51..179F, 1983A&AS...52..411F) p: detected by Douglas et al. (1973AJ.....78....1D) q: B2 position (Colla et al., 1972A&AS....7....1C) s: NE component of 4CP66.16.1 u: data for outer part v: data for central part ':' : uncertainty flag --- PA Position angle of the major axis deg n_PA Uncertainty flag on PA :)?=uncertainty flag, C=complex, r: resolved --- e_PA rms uncertainty on PA deg l_MajAxis Limit flag on MajAxis --- MajAxis Deconvolved half width along major axis arcmin n_MajAxis C=complex, : uncertainty flag --- l_MinAxis Limit flag on MinAxis --- MinAxis Deconvolved half width along minor axis arcmin n_MinAxis C=complex, : uncertainty flag --- l_m Limit flag on m --- m Integrated degree of linear polarization % u_m Uncertainty flag on m --- e_m rms uncertainty on m % n_m Note on m number=4 ':' : uncertainty flag f: main contribution from NW component c: main contribution from SW part of source --- Xi Integrated polarization position angle of electric field vector deg e_Xi rms uncertainty on Xi deg u_Xi Uncertainty flag on Xi --- l_Pdist Limit flag on Pdist --- Pdist Projected distance of source to the cluster center in units of one Abell radius --- u_Pdist Uncertainty flag on Pdist --- l_P2.7 Limit flag on P2.7 --- P2.7 Spectral power at 2.7GHz assuming cluster membership --- n_P2.7 : = uncertainty flag, a = redshift taken from A2319A, see table2e --- IdOpt Optical identification --- OptCl Optical class --- n_IdOpt Note on ref file number=5 E: the following references are in ref2e file D: the following references are in ref2d file G: the following references are in ref2g file T: the following references are in ref2t file --- r_IdOpt Reference for optical data --- MemCl Membership class --- l_SpI Limit flag on SpI --- SpI Average spectral index --- u_SpI Uncertainty flag on SpI --- e_SpI rms uncertainty on SpI --- SpCl Spectral class number=6 S: straight power law C+: concave C-: convex Cmax: low frequency turnover C: complex --- n_Ref note for ref file number=5 E: the following references are in ref2e file D: the following references are in ref2d file G: the following references are in ref2g file T: the following references are in ref2t file --- Ref Radio references number=5 E: the following references are in ref2e file D: the following references are in ref2d file G: the following references are in ref2g file T: the following references are in ref2t file --- 6.3cm (4.75GHz) radio data (Papers 5, 6 and 7) Source Source name number=1 For the reobserved fields, the nomenclature is consistent with previous papers, except for A1060 and A2199, for which a renumbering was necessary. --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s NotePos Note on position number=2 a) 11 cm position b) position from 2.8 cm map c) position from Harris et al. (1980A&AS...39..215H) --- DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec u_Pos Uncertainty flag on B1950 position --- l_S4.75GHz Limit flag on S4.75GHz --- S4.75GHz Flux density at 4.75GHz (6.3cm) mJy e_S4.75GHz rms uncertainty on S4.75GHz mJy n_S4.75GHz Note on S4.75GHz number=3 a) excluding EW extension --- rmsI rms noise level at 2.7GHz in total intensity (in mJy/beam area) mJy rmsP rms noise level at 2.7GHz in polarized intensity (in mJy/beam area) mJy PA Position angle of major axis of extended sources deg n_PA C = complex, : uncertainty flag --- l_MajAxis Limit flag on MajAxis --- MajAxis Deconvolved half width along major axis arcmin n_MajAxis C = complex, r = resolved, : uncertainty flag --- l_MinAxis Limit flag on MinAxis --- MinAxis Deconvolved half width along minor axis arcmin n_MinAxis C = complex, r = resolved, : uncertainty flag --- l_m Limit flag on m --- m Integrated degree of linear polarization % e_m rms uncertainty on m % Xi Integrated polarization position angle of electric field vector deg e_Xi rms uncertainty on Xi deg Pdist Projected distance --- l_P4.75 Limit flag on P4.75 --- P4.75 Spectral power at 4.75GHz assuming cluster membership --- 6.2cm (4.85GHz) radio data (Paper 3) Source Source name number=1 We have labelled each prominent source with a subnumber (A85.1 etc.), regardless of cluster membership, in increasing order of right ascension for each cluster area mapped. We have only labelled the most prominent sources. For sources appearing complex at 11.1cm (Paper I (1978A&AS...31...99H or II1979A&AS...36..237W), and being resolved by the present observation, we preserved the subnumbering already given to the source and distinguished the subcomponents by small letters following the subnumber (A407.4a etc.). --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec u_Pos Uncertainty flag on position --- l_S4850MHz Limit flag on S4850MHz --- S4850MHz Flux density at 4850 MHz mJy u_S4850MHz Uncertainty flag on S4850MHz --- e_S4850MHz rms uncertainty on S4850MHz mJy rms rms noise level of the cluster map, calculated for areas where there are no sources (in mJy/beam area) --- PA Position angle of the major axis of extended sources deg u_PA Uncertainty flag on PA --- l_MajAxis Limit flag on MajAxis --- MajAxis Half-power width along major axis arcmin u_MajAxis Uncertainty flag on MajAxis --- l_MinAxis Limit flag on MinAxis --- MinAxis Half-power width along minor axis arcmin u_MinAxis Uncertainty flag on MinAxis --- d/R Projected distance (ratio of distance from the cluster center to the Abell radius) in units of Abell radius --- l_SpI Limit flag on SpI --- SpI Mean spectral index between 600 and 4800MHz --- u_SpI Uncertainty flag on SpI --- SpCl Classification of the radio spectrum number=2 S: straight spectra C-: convex spectra Cmax: spectra showing a low-frequency cut-off C+l: concave spectra with low-frequency excess C+s: concave spectra with high-frequency excess CPX: complex spectra --- CatName Catalogue names for the different cluster sources or the cluster as a whole as taken from the available literature --- Ref References (see ref3 file) --- 2.8cm (10.7GHz) radio data (Paper 5 and 6) Source Source name number=1 We have labelled each prominent source with a subnumber (A85.1 etc.), regardless of cluster membership, in increasing order of right ascension for each cluster area mapped. We have only labelled the most prominent sources. --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec NotePos a: peak positions only, : uncertainty flag --- l_S10.7GHz Limit flag on S10.7GHz --- S10.7GHz Flux density ar 10.7GHz (2.8cm) mJy e_S10.7GHz rms uncertainty on S10.7GHz mJy n_S10.7GHz Note on S10.7GHz number=2 b) includes contribution from surrounding emission feature c) possibly variable, flux at epoch 1979.7 was 180 mJy --- rmsI rms noise level at the maps area which - bona fide - do not contain radio sources (in mJy/beam area) mJy rmsP rms noise level in linearly polarized intensity (in mJy/beam area) mJy PA Position angle of the major axis of extended sources deg u_PA Uncertainty flag on PA (C=complex) --- l_MajAxis Limit flag on MajAxis --- MajAxis Major axis half power width arcmin u_MajAxis Uncertainty flag on MajAxis (C=complex) --- l_MinAxis Limit flag on MinAxis --- MinAxis Minor axis half power width arcmin u_MinAxis Uncertainty flag on MinAxis (C=complex) --- l_m Limit flag on m --- m Integrated degree of linear polarization % u_m Uncertainty flag on m --- e_m rms uncertainty on m % Xi Weighted mean of the electric field vector position angle deg e_Xi rms uncertainty on Xi deg u_Xi Uncertainty flag on Xi --- Note Note --- r2700a file references r2700b file references (D series) r2700b file references (E series) r2700b file references (G series) r2700b file references (T series) r4850 file references clopx file references clparam file references RefNo Reference number --- BibCode Bibcode --- Authors List of the authors --- Patricia Bauer, Francois Ochsenbein CDS 1997 Nov 28 It is a pleasure to thank Heinz Andernach <heinz@polaris.astro.ugto.mx> who kindly supplied his data to CDS. UNKNOWN UNKNOWN The data were supplied by Heinz Andernach (catalog A043 in his list). A few annex tables (clopt, clopx, ref4 and 5) were prepared via OCR at CDS. VIII_43.xml The Miyun 232 MHz survey. II. The main list 8044 VIII/44 Miyun 232MHz survey The Miyun 232 MHz survey. II. The main list X Zhang Y Zheng H Chen S Wang A Cao B Peng R Nan Astron. Astrophys. Suppl. Ser. 121 59 1997 1997A&AS..121...59Z VIII/18 : 6C Survey at 151MHz (I) (Baldwin+ 1985) VIII/21 : 6C Survey at 151MHz (II) (Hales+ 1988) VIII/22 : 6C Survey at 151MHz (III) (Hales+ 1990) VIII/23 : 6C Survey at 151MHz (IV) (Hales+ 1991) VIII/24 : 6C Survey at 151MHz (V) (Hales+ 1993) VIII/25 : 6C Survey at 151MHz (VI) (Hales+ 1993) Zhang X. et al., 1993A&AS...99..545Z: The Miyun 232 MHz survey. I. Radio sources surveys catalogs radio continuum: general A meter-wave survey of the sky region north of declination +30{deg} has been carried out with the Miyun Synthesis Radio Telescope (MSRT), Beijing Astronomical Observatory, at 232MHz. It is a moderately deep survey. The observations were made between January 1985 and December 1993. The covered sky area is divided into 156 fields of view. Basically all adjacent fields are separated by 8 degree angular distance. Fields #54, #56, #115, #116, have no data yet. A catalog of 34462 radio sources is given in Table 2. Table3 shows the information on the 152 fields of view.
The source-list of the survey Name Source name number=1 The name is based on a truncated B1950 position; a suffix A, B, C or D differentiates sources with identical truncated positions. --- RAh Right ascension 1950.0 of the source h RAm Right ascension 1950.0 of the source min RAs Right ascension 1950.0 of the source s DEd Declination 1950.0 of the source deg DEm Declination 1950.0 of the source arcmin DEs Declination 1950.0 of the source arcsec Speak Peak flux density (Jy/beam) Jy Sint Integrated flux density (Jy/beam) Jy Factor Factor for correcting the primary beam --- S/N Local S/N number=2 Local S/N is calculated in the way of maximum (peak flux, integral flux)/(local noise) --- Field Number of the field of view --- Information on 152 fields of view Field Number of the field of view --- RAh Right ascension of the field center at OBSdate h RAm Right ascension of the field center at OBSdate min RAs Right ascension of the field center at OBSdate s DEd Declination of the field center at OBSdate deg OBSdate Observing date DD/MM/YY Fluct Background fluctuation (mJy/beam) mJy fig1.ps Arrangement of the fields in the Miyun 232MHz survey fig2.ps Comparisons of flux densities fig3.ps *rms of background fluctuation in RA direction fig4.ps *rms of background fluctuation in DE direction Patricia Bauer CDS 1996 Jun 03 Xizhen Zhang <zxz@bao01.bao.ac.cn> VIII_44.xml The Maryland-Green Bank Galactic 21-cm line survey 8047 VIII/47 Galactic 21-cm line Survey The Maryland-Green Bank Galactic 21-cm line survey G Westerhout H U Wendlandt Astron. Astrophys. Suppl. 49 137 1982 1982A&AS...49..137W H I data Surveys Galactic plane Atlases This catalog presents a completely sampled survey of 21-cm line profiles extending from Galactic longitude 11 to 235 degrees and nominally covering a range between latitude +2 and - 2 degrees. It was observed in 1971-72 with the newly resurfaced 92-m (300-foot) telescope of the National Radio Astronomy Observatory (NRAO) in Green Bank, W.V. The spatial resolution is 0.22 degrees (13 arcmin), and the velocity resolution is 2 km/s. The line profiles have 260 values of Brightness Temperature at 1 km/s intervals, and at spacings of 0.1 degree in longitude and 0.1 degree in latitude. The r.m.s per data point varies from 1.0K at low declinations to 0.5K at high declinations. The maps at constant Galactic longitude published in the printed version are at intervals of 0.2 degrees in longitude; the spectra in this catalog are therefore spatially twice as dense. The catalog is arranged in two forms: as FITS data cubes, and as FITS binary tables. The cubes contain three-dimensional arrays of spectra for various longitude ranges. The binary tables contain spectra at constant Galactic latitude, along with coordinate and velocity information necessary for the interpretation of individual spectra. A detailed description of the telescope beam characteristics and the derivation of the temperature scale is given by Westerhout, G., Mader, G.L., and Harten, R.H. (Astron. and Astrophys. Suppl. 49, 137-141, 1982). Temperature scales of this and several other 21-cm line surveys were compared by Harten, R.H., Westerhout, G., and Kerr, F.J. (Astron.J. 80, 307-310, 1975) and found to agree to within 5 %.
l011_020.fit FITS cubes for l = 11.0-19.9 deg l020_040.fit l = 20.0-39.9 deg l040_060.fit l = 40.0-59.9 deg l060_080.fit l = 60.0-79.9 deg l080_100.fit l = 80.0-99.9 deg l100_120.fit l = 100.0-119.9 deg l120_140.fit l = 120.0-139.9 deg l140_160.fit l = 140.0-159.9 deg l160_180.fit l = 160.0-179.9 deg l180_200.fit l = 180.0-199.9 deg l200_220.fit l = 200.0-219.9 deg l220_235.fit l = 200.0-235.0 deg b_m22.fit FITS tables for b = -2.2 deg b_m21.fit b = -2.1 deg b_m20.fit b = -2.0 deg b_m19.fit b = -1.9 deg b_m18.fit b = -1.8 deg b_m17.fit b = -1.7 deg b_m16.fit b = -1.6 deg b_m15.fit b = -1.5 deg b_m14.fit b = -1.4 deg b_m13.fit b = -1.3 deg b_m12.fit b = -1.2 deg b_m11.fit b = -1.1 deg b_m10.fit b = -1.0 deg b_m09.fit b = -0.9 deg b_m08.fit b = -0.8 deg b_m07.fit b = -0.7 deg b_m06.fit b = -0.6 deg b_m05.fit b = -0.5 deg b_m04.fit b = -0.4 deg b_m03.fit b = -0.3 deg b_m02.fit b = -0.2 deg b_m01.fit b = -0.1 deg b_00.fit b = 0.0 deg b_01.fit b = 0.1 deg b_02.fit b = 0.2 deg b_03.fit b = 0.3 deg b_04.fit b = 0.4 deg b_05.fit b = 0.5 deg b_06.fit b = 0.6 deg b_07.fit b = 0.7 deg b_08.fit b = 0.8 deg b_09.fit b = 0.9 deg b_10.fit b = 1.0 deg b_11.fit b = 1.1 deg b_12.fit b = 1.2 deg b_13.fit b = 1.3 deg b_14.fit b = 1.4 deg b_15.fit b = 1.5 deg b_16.fit b = 1.6 deg b_17.fit b = 1.7 deg b_18.fit b = 1.8 deg b_19.fit b = 1.9 deg b_20.fit b = 2.0 deg b_21.fit b = 2.1 deg b_22.fit b = 2.2 deg b_23.fit b = 2.3 deg b_24.fit b = 2.4 deg Gart Westerhout retired 1997 Jun 10 UNKNOWN UNKNOWN At the edges of the survey, near l=11 to 12.5 degrees and l=233.5 to 235 degrees, not all Galactic longitudes for a given latitude were measured, so that cross sections at constant b have gaps in l. Near l=60, b=-1.5 to -1.7 and l= 64 to 66, b=+1.7 to +2.4 the survey coverage in b widens from 3.2 to 4.7 degrees. Over most of the range l=12 to 234 the survey covers a strip of 4.5 degrees in Galactic latitude centered on the Galactic plane. In more detail, the survey covers the following longitudes and latitudes: >From l=11.0 to l= 64.1, b=+1.7 and l= 12.5 to l= 59.7, b=-1.5 >From l=64.2 to l=235.0, b=+2.4 and l= 59.8 to l=131.9, b=-2.2 and l=132.0 to l=233.2, b=-1.9 VIII_47.xml The Zelenchuk survey 3.9 GHz Survey (0 to 14 degs) 8049 VIII/49 The Zelenchuk Surveys The Zelenchuk survey 3.9 GHz Survey (0 to 14 degs) V R Amirkhanyan The Zelenchuk 3.9 GHz Survey ??? ??? 1989 1989 The Zelenchuk survey 3.9 GHz Survey (0 to 14 degs) M G Larionov Soobshch. Spets. Astrof. Obs. 68 14 1991 1991SoSAO..68...14L The Zelenchuk survey 3.9 GHz Survey (0 to 14 degs) M G Larionov Yu N Parijskij V I Zhuravlev V N Sidorenkov A B Berlin N A Nizhel'skii Astron. Astrophys. Suppl. Ser. 106 119 1994 1994A&AS..106..119L The Zelenchuk survey 3.9 GHz Survey (0 to 14 degs) V R Amirkhanyan A G Gorshkov A A Kapustkin V K Konnikova A N Lazutkin Pis'ma Astron. Zh. 18 396 1992 1992PAZh...18..396A The Zelenchuk survey 3.9 GHz Survey (0 to 14 degs) V R Amirkhanyan A G Gorshkov V K Konnikova Astron. Zh. 69 225 1992 1992AZh....69..225A J/A+AS/87/1 : Parijskij et al, 1991, RATAN-600 7.6 cm catalog of radio sources from "Experiment Cold-80" J/AZh/72/291 : Variabilities at 3.9 and 7.5GHz (Gorshkov+ 1995) Radio sources Surveys The main catalog contains positions and flux densities for 8511 sources detected in the Zelenchuk 3.9 GHz Survey with declinations between 0 and 14 degrees. The survey was originally published in Amirkhanyan et al. 1989, MIR Publ., Moscow, and contained 8511 sources. The machine version has been cleaned from a few spurious sources by the authors. The angular resolution is (RA x DEC) 70"/cos(decl) x 50'. The survey is 95 percent complete to the limiting flux density 50 mJy, except near the boundaries of the declination zone. A supplementary catalogue of 2946 radio sources observed during Zelenchuk survey at 3.9 GHz in the flux density from 40 to 50 mJy within the declination range 0-14 degrees are presented. ratan is the first results of the deep search survey over a portion of the celestial sphere with the radio telescope RATAN-600 at several cm-wavelengths. The catalogue contains 691 radio sources at 3.9 GHz. Fluxes at the frequencies 3.9, 4.8, 7.5 and 11.2 GHz have been measured for the complete sample of the radio sources from the Zelenchuk survey. The sample contains all sources with S > 200 mJy in the 4-6 degree declination range.
Radio survey at 3.9 GHz decl. 0-14deg Name Object name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) number=1 In the catalogue, the declination was given only as hours and minutes, due to the sparse resolution in declination. A rough approximation to positional errors is d(DEC) ~ 0.45'/S[Jy] arcmin RA2000h Right Ascension 2000 (hours) h RA2000m Right Ascension 2000 (minutes) min RA2000s Right Ascension 2000 (seconds) s DE2000- Declination 2000 (sign) --- DE2000d Declination 2000 (degrees) deg DE2000m Declination 2000 (minutes) number=1 In the catalogue, the declination was given only as hours and minutes, due to the sparse resolution in declination. A rough approximation to positional errors is d(DEC) ~ 0.45'/S[Jy] arcmin S3.9GHz Peak flux density at 3.9 GHz number=2 A crude estimate of the flux density error is dS = sqrt((0.1)**2 +(S/10Jy)**2 ) Jy The errors in flux density and position may be estimated using the following table: Flux S(Jy) Error S(mJy) dPA cosD (sec) dD (') -------------------------------------------------------- 0.05 11 0.67 9.1 0.07 12 0.50 6.5 0.10 14 0.37 4.6 0.20 22 0.24 2.3 0.30 32 0.21 1.5 0.40 41 0.20 1.1 0.50 51 0.20 0.9 0.70 71 0.19 0.7 1.00 100 0.19 0.5 -------------------------------------------------------- where dPA is the difference in right ascension, cosD is the cosine ascension, and dD is the difference in declination." mJy OtherName Other name number=3 This column gives an alternative name for the source, taken from Dixon's Master List of Radio Sources, 1977 (Cat. <VII/2>), Astron.Tsirk. 1099,2; Astron.Tsirk. 1137,5; Astron.Tsirk. 1157,2, Astron.Zhurn. 58,717; Large et al 1981, MNRAS 194,693 (Cat. <VIII/16>) AuJP 35,177; ApJS 51,67; ApJS 61,1 (the MIT-Green Bank (MG I) survey). --- Weak sources at 3.9 GHz decl. 0-14deg Name Source designation --- m_Name Possible component --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Sign of declination (1950) --- DEd Declination (1950) number=1 For source 0701+039, the printed declination is +03 5 .8 deg DEm Declination (1950) arcmin S3.9GHz 3.9 GHz peak flux density mJy 3.9GHz survey decl. -1 to 0 deg (Table 2 of paper 1994A&AS..106..119L) [LPZ94] Sequential number number=1 Sequential number as in Table 2 of paper by Larionov et al., in 1994A&AS..106..119L --- Name Source name (RATAN) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin S3.9GHz Flux density at 3.9 GHz mJy e_S3.9GHz rms uncertainty of S3.9GHz (5*rms) mJy Other Other name --- Survey of the polar region at 3.9GHz Name Source name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DEd Declination 1950 deg DEm Declination 1950 arcmin S3.9GHz Flux density at 3.9 GHz mJy e_S3.9GHz rms uncertainty of F3.9GHz (5*rms) mJy Other Other name --- Complete sample of the radio sources at 3.9, 4.8, 7.5 and 11.2 GHz Name Source name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec S3.9GHz Flux density at 3.9 GHz mJy e_S3.9GHz rms uncertainty of S3.9GHz (5*rms) mJy S4.8GHz Flux density at 4.8 GHz mJy e_S4.8GHz rms uncertainty of S4.8GHz (5*rms) mJy S7.5GHz Flux density at 7.5 GHz mJy e_S7.5GHz rms uncertainty of S7.5GHz (5*rms) mJy S11.2GHz Flux density at 3.9 GHz mJy e_S11.2GHz rms uncertainty of S11.2GHz (5*rms) mJy Francois Ochsenbein CDS Veta Avedisova INASAN 1997 Nov 06 It is a pleasure to thank H. Andernach <Heinz.Andernach@astro.ugto.mx> who forwarded a copy of his electronic version to CDS. UNKNOWN UNKNOWN * File main.dat was provided by V. Konnikova (Moscow) to H. Andernach in July 1994 * File suppl.dat was provided by M.G. mgl@sai.msu.su to H. Andernach in March 1996; it was also independently prepared at CDS. * File ratan.dat was received on diskette from A&A Editors (March 1994) and distributed as table2 of catalog J/A+AS/106/119 ; the "[LPZ94]" column (sequential number) was added (November 1995) * File polar.dat was provided by Vladimir Amirchkanjan <amir@sao.stavropol.su> to H. Andernach in March 1993 * File sample.dat was provided by Vladimir Amirchkanjan <amir@sao.stavropol.su> to H. Andernach in May 1995 * On 27-Nov-1997, suppl.dat file was corrected VIII_49.xml The FIRST Survey Catalog of 1.4GHz radio sources 8051 VIII/51 the FIRST Survey, version 1998Feb The FIRST Survey Catalog of 1.4GHz radio sources R L White R H Becker D J Helfand M D Gregg Astrophys. J. 475 479 1998 1997ApJ...475..479W http://sundog.stsci.edu/ : home page of the VLA FIRST Survey http://sundog.stsci.edu/first/catalogs/history.html : Version History http://sundog.stsci.edu/cgi-bin/searchfirst : the FIRST search engine http://third.llnl.gov/cgi-bin/firstcutout : the FIRST Cutout Server. http://www.cv.nrao.edu/first/ : FIRST page at NRAO Radio sources Surveys The FIRST survey to produce Faint Images of the Radio Sky at Twenty centimeters began in 1993. It uses the VLA (Very Large Array, a facility of the National Radio Observatory (NRAO)) at a frequency of 1.4GHz, and it is slated to 10,000 deg^2^ to a sensitivity of about 1mJy with an angular resolution of about 5". The co-added images are available on the Internet (see the FIRST home page at http://sundog.stsci.edu/ for details). The source catalogue is derived from the images. This version of the FIRST Survey is derived from the 1993 through 1997 observations, and contains 382,892 sources for the north Galactic cap, and 54,537 sources for the south Galactic cap. The northern catalog covers about 4150 square degrees of sky, including most of the area: 7h20m < RA(2000) < 17h20m 22.2{deg} < Dec < 57.6{deg} The southern catalog covers about 610 square degrees of sky, including two narrow strips in the area 21h20m < RA(2000) < 3h20m -11.5{deg} < Dec < 1.6{deg}
North Galactic Cap (7h20<RA<17h20, +22.2{deg}<Dec<+57.6{deg}) South Galactic Cap (21h20<RA<3h20, -11.5{deg}<Dec<+01.6{deg}) FIRST FIRST Source designation This column (not part of the original catalog) contains the source name built from the rule registered at IAU ('J' followed by truncated J2000-position) --- RAh Right Ascension J2000 (hours) Position position (J2000) of the source. The accuracy of the position depends on the brightness and size of the source and the noise in the map. Point sources at the detection limit of the catalog have positions accurate to better than 1 arcsec at 90% confidence; 2 mJy point sources in typically noisy regions have positions good to 0.5 arcsec. An empirical expression for the positional accuracy is unc(90% confidence) = Size (1/SNR + 1/20) arcsec where Size is either the major or minor axis fitted FWHM (fMaj or fMin) as given in the catalog and SNR is the peak flux density signal-to-noise ratio: SNR = (Fpeak-0.25) / Rms (The positional uncertainty is of course elliptical for elliptical sources.) The best possible positional uncertainty is limited to about 0.1 arcsec by our ability to fit source positions in maps with 1.8 arcsec pixels and by various random calibration uncertainties. Systematic errors in the positions are smaller than 0.05 arcsec. h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Wflag Warning flag `W' is a warning flag indicating that the source may be a sidelobe of a nearby bright source. In the northern catalog, 14,039 sources (3.7%) are flagged as possible sidelobes; in the southern catalog, 1,943 sources (3.6%) are flagged as possible sidelobes. The flagging algorithm is an artificial intelligence approach based on oblique decision trees. Our analysis indicates that <10% of the objects flagged as sidelobes are real sources and that considerably less than 1% of the unflagged sources in the catalog are sidelobes. Complete details of the sidelobe identification procedure are included in our catalog paper. NOTE: The sidelobe flagging in the southern catalog may not be as reliable as in the north because the sidelobe characteristics change with the zenith angle of the observation. We are working on improvements to the sidelobe-flagging, but for now it is important to be cautious in studies of individual southern sources. We recommend checking the images using the FIRST Cutout Server if there is any doubt about the reality of particular sources (in either the north or the south.) This is easily done when using the FIRST Search Engine to search the catalog, since each source selected in the search has a link to the Cutout Server. --- Fpeak Peak flux density at 1.4GHz Fpeak and Fint are the peak and integrated flux densities measured in mJy. They are derived by fitting an elliptical Gaussian model to the source. To correct for the ``CLEAN bias'' effect, 0.25 mJy has been added to the peak flux density and the integrated flux density has been multiplied by (1+0.25/Fpeak) (see our Astrophysical Journal paper and our catalog paper for more details.) The uncertainty in Fpeak is given by the rms noise at the source position, while the uncertainty in Fint can be considerably greater depending on the source size and morphology. For bright sources the accuracies of Fpeak and Fint are limited to about 5% by systematic effects. Note that for sources that are not well-described by an elliptical Gaussian model, Fint is not an accurate measure of the integrated flux density. mJy Fint Integrated flux density at 1.4GHz mJy Rms Local noise estimate Rms is a local noise estimate at the source position measured in mJy. Rms is computed by combining the measured noise from all grid pointing images contributing to this coadded map position. Note that the significance of detection for a source is (Fpeak-0.25)/Rms, not Fpeak/Rms, because of the CLEAN bias correction to the peak flux density. The catalog includes only sources brighter than 5 Rms. FITS images giving the rms noise as a function of position on the sky are available for the northern and the southern areas. These images give the rms in mJy/beam tabulated on a ~3 arcmin grid in RA and Declination. If there is no source in the catalog at a given position, the source peak flux density (before CLEAN bias correction) is less than 5 times the coverage map rms value at that position. mJy MajAxis Major axis (FWHM) MajAxis, MinAxis, and PA give the major and minor axes (FWHM in arcsec) and position angle (degrees east of north) derived from the elliptical Gaussian model for the source. MajAxis and MinAxis have been deconvolved to remove blurring by the elliptical Gaussian point-spread function. (The fitted parameters before deconvolution are given in the fMaj, fMin, and fPA columns.) In the north the beam is circular 5.4 arcsec FWHM; in the south it is elliptical, 6.4x5.4 arcsec FWHM, with the major axis running north-south. Noise can cause the fitted values of the major and minor axes (before deconvolution) to be smaller than the beam. The corresponding deconvolved size is given as zero in those cases. The uncertainties in the deconvolved sizes depend on both the brightness and the sizes. Objects at the catalog flux density limit have uncertainties of about 2 arcsec in their sizes (so faint objects with Maj < 2 arcsec are consistent with point sources.) An simple empirical estimate of the uncertainty is Sigma(Size) = 10 arcsec (1/SNR + 1/75) where SNR is the signal-to-noise ratio defined above. arcsec MinAxis Minor axis (FWHM) arcsec PA Position angle deg fMaj Fitted MajAxis before deconvolution fMaj, fMin, and fPA give the major and minor axes (FWHM in arcsec) and position angle (degrees east of north) derived from the elliptical Gaussian model for the source. These are the fitted sizes measured directly from the image; the elliptical point-spread function has not been deconvolved. arcsec fMin Fitted MinAxis before deconvolution arcsec fPA Fitted PA before deconvolution deg Field Name of the coadded image containing the source The Field Name is the name of the coadded image containing the source. Note that the field name encodes the position of the field center: field hhmmm+ddmmm is centered at RA=hh mm.m, Dec=+dd mm.m. The images are available from several archives and through the FIRST Cutout Server. All field names in the current catalog end with E or F, indicating that they were constructed using the imaging pipeline that applies a small rotation and scale correction. See the catalog history page for more information. The F fields are new in this catalog, while sources extracted from the E fields are identical to those in the previous version of the catalog. Some E fields from the last catalog have been replaced by new F fields because there were additional grid images available for the coadding. --- Richard L. White STScI 1998 Feb 04 UNKNOWN UNKNOWN The files (originally catalog_north_98feb04.bin and catalog_south_98feb04.bin) were copied from http://sundog.stsci.edu/first/catalogs/readme.html The preceding version (1997 April 24) was numbered <VIII/48> in CDS Archives. See http://sundog.stsci.edu/first/catalogs/history.html for the complete version history. VIII_51.xml The MIT-Green Bank (MG) 5 GHz survey 8052A VIII/52A The MIT-Green Bank 5GHz Survey The MIT-Green Bank (MG) 5 GHz survey C L Bennett C R Lawrence B F Burke J N Hewitt J Mahoney Astrophys. J. Suppl. Ser. 61 1 1986 1986ApJS...61....1B The MIT-Green Bank (MG) 5 GHz survey G I Langston M B Heflin S R Conner J Lehar C L Carrilli B F Burke Astrophys. J. Suppl. Ser. 72 621 1990 1990ApJS...72..621L The MIT-Green Bank (MG) 5 GHz survey M Griffith G Langston M Heflin S Conner J Lehar B Burke Astrophys. J. Suppl. Ser. 74 129 1990 1990ApJS...74..129G The MIT-Green Bank (MG) 5 GHz survey M Griffith G Langston M Heflin S Conner B Burke Astrophys. J. Suppl. Ser. 75 801 1991 1991ApJS...75..801G VIII/14 : 87GB Radio Sources 4.85 GHz (Gregory, Condon 1991) A 4.85 GHz sky survey. (Condon+ 1994) =1994AJ....107.1829C 90GB 4.85 GHz Sky Maps (Condon+ 1995) =1995ADIL...JC...06C Condon, J. J., and Broderick, J. J. 1985, AJ, 90, 2540 =1985AJ.....90.2540C Douglas, J. N., Bash, F. N., Torrence, G. W., and Wolfe, C. 1980, The Texas Survey: Preliminary +18 deg Strip (Univ. Texas Pub. Astr. No. 17). =1980PAUTx..17....1D Radio continuum Radio sources radio sources: general radio sources: identifications The MIT-Green Bank 5 GHz survey catalog was produced from four separate surveys with the National Radio Astronomy Observatory (NRAO) 91m transit telescope (Bennett et al., 1986ApJS...61....1 (MG1); Langston et al., 1990ApJS...72..621 (MG2); Griffith et al., 1990ApJS...74..129 (MG3); Griffith et al. 1991ApJS...75..801 (MG4)). The sky coverage of the various surveys is 00h < RA < 24h, -00d30'13" < DECB < +19d29'47" for MG1; 04h < RAJ < 21h, +17.0d < DECJ < +39d09' for MG2; 16h30m < RAB < 05h, +17d < DECB < +39d09' for MG3; and 15h30m < RAB < 02h30m; +37.00d < DECB < +50d58'48" for MG4; where RAB and DECB refer to B1950 coordinates, and RAJ and DECJ refer to J2000 coordinates. The catalog contains 20344 sources detected with a signal-to-noise ratio greater than 5 and 3836 possible detections (MG1) with a signal-to-noise ratio less than 5. Spectral indices are computed for MG1 sources also identified in the Texas 365 MHz survey (Douglas et al. 1980), and for MG1-MG4 sources also identified in the NRAO 1400 MHz Survey (Condon and Broderick 1985). Notice: Original names were expanded by H.Andernach to MGn_Jhhmmss+ddmm, as suggested by Glen Langston on 25-Mar-1998 in reply to an inquiry by the IAU TG on Designations.
MG1-4 source list Name Source name sources with signal-to-noise ratios less than 5 are listed as 'MG1s...' --- RAh right ascension B1950 h RAm right ascension B1950 min RAs right ascension B1950 s DE- declination sign --- DEd declination B1950 deg DEm declination B1950 arcmin DEs declination B1950 arcsec l_Flux Flux density limit flag blank if 'Flux' is actual flux density '>' if 'Flux' is lower limit on flux density (MG1 fluxes over 5 Jy are listed as "> 5000" due to receiver saturation.) --- Flux Green Bank flux density at 4.830 or 4.775 GHz mJy n_Flux Flux note flag blank if frequency is 4.830 GHz (MG2-4) '*' if frequency is 4.775 GHz (MG1) --- l_S/N Signal-to-noise limit flag blank if 'S/N' is actual signal-to-noise '>' if 'S/N' is lower limit on signal-to-noise (MG1 S/N values over 100 are listed as ">99.9".) --- S/N Signal-to-noise ratio of the detection, or lower limit on signal-to-noise. --- G Group containing the source G is defined by the north or south survey detecting the source and the source location in the survey. Sources with b > +10 deg and detected in the south, north, or both surveys are assigned to groups 0, 1, 2. Sources lying in regions observed only once or at low Galactic latitude |b| < 10 deg, and detected in the south, north, or both surveys are assigned to groups 3, 4, or 5. Sources in the region observed twice but with b < -10 deg and detected in south, north, or both surveys, are assigned to groups 6, 7, or 8. --- alpha The spectral index of the source, where Flux {prop.to.} {nu}^alpha^ --- n_alpha Spectral index note flag blank if spectral index derived using NRAO 1400 MHz and 4.830 GHz observations (MG2-4) "*" if derived using Texas 365 MHz and 4.775 GHz observations (MG1) --- Tom Sodroski SSDOO/ADC 1999 Apr 30 This catalog was originally compiled by Dr. Heinz Andernach at the Universidad de Guanajuato. VIII_52A.xml A Green Bank sky survey in search of radio sources at 1400 MHz. III. Positions and flux densities of the GB radio sources. 8053 VIII/53 The Green Bank Survey A Green Bank sky survey in search of radio sources at 1400 MHz. III. Positions and flux densities of the GB radio sources. J Maslowski Acta Astron. 22 227 1972 1972AcA....22..227M A Green Bank sky survey in search of radio sources at 1400 MHz. III. Positions and flux densities of the GB radio sources. J Machalski Acta Astron. 28 367 1978 1978AcA....28..367M A Green Bank sky survey in search of radio sources at 1400 MHz. III. Positions and flux densities of the GB radio sources. S Rys J Machalski Acta Astron. 37 163 1987 1987AcA....37..163R Radio continuum Radio sources Surveys This catalog presents the parts I, II, and III of the Green Bank survey of extragalactic radio sources at 1400 MHz. The data were obtained with the 300' antenna, producing a beamwidth of 10'x11' FWHM. Part I of the survey covers about 521 square degrees of the sky with RA from 7h17m to 16h23m, DEC from +45.8{deg} to +51.7{deg}. 1086 sources are presented down to a limiting flux density of 90 mJy. These data were originally published in Maslowski, 1972, Acta Astronomica, 22, 227 (1972AcA....22..227M). Part II of the survey covers 0.28 sr of the sky with RA from 7h08m to 16h57m, DEC from +31.9{deg} to +39.7{deg}. 2022 sources are presented down to a limiting flux density of 0.09 mJy. Spectral indices between 1400 MHz and 408 MHz are determined for most sources by comparison with the B2 source catalog (Cat.<VIII/36>). These data were originally published in Machalski 1978, Acta Astronomica, 28, 367 (1978AcA....28..367M) Part III of the survey covers an area of 0.099 sr at declinations between 70 and 76.8 degrees. This catalog contains a total of 676 radio sources, of which 502 are statistically complete to 112 mJy. These data were originally published as Rys and Machalski, 1987, Acta Astronomica, 37, 163 (1987AcA....37..163R).
Green Bank I Survey at 1400 MHz (Dec: 45d to 52d) Green Bank II Survey at 1400 MHz (Dec: 32d to 40d) Green Bank III Survey at 1400 MHz (Dec: 70d to 77d) Name Coordinate-designated B1950 name number=1 This column contains the name of the source, derived from its B1950 coordinates. Names have been designated with a 'GBx', where 'x' is 1 , 2, or 3, followed by the hours and minutes of RA, declination sign, then degrees and truncated minutes (e.g. 'GB2 0714+384'). For a few objects close to each other, a duplication of names was avoided by appending an "A" or "B" to the name. --- RAh Right Ascension (B1950) (hour) number=2 These columns give the B1950 coordinates of the source, in degrees and in radians. Positional uncertainties for GB3 in RA and DEC are estimated to be: ra_err = +/-[(0.45)^2^ + (120/S)^2^]^1/2^ arcmin dec_err = +/-[(0.39)^2^ + (165/S)^2^]^1/2^ arcmin where flux density S is expressed in mJy. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=2 These columns give the B1950 coordinates of the source, in degrees and in radians. Positional uncertainties for GB3 in RA and DEC are estimated to be: ra_err = +/-[(0.45)^2^ + (120/S)^2^]^1/2^ arcmin dec_err = +/-[(0.39)^2^ + (165/S)^2^]^1/2^ arcmin where flux density S is expressed in mJy. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec pos_flg Flagged '?' if position is less certain number=3 pos_flg is flagged with a colon ':' if the position is less certain. In these cases the positional uncertainty is larger than that expressed above. --- S1400 Integrated 1400 MHz flux density in Jy number=4 The integrated 1400 MHz flux is given in the S1400 column, in Jy. The u_S1400 column is marked with a colon ':' if the integrated flux is uncertain. The S1400p column gives the peak 1400 MHz flux density, when known. Jy u_S1400 ':' if flux is less certain number=4 The integrated 1400 MHz flux is given in the S1400 column, in Jy. The u_S1400 column is marked with a colon ':' if the integrated flux is uncertain. The S1400p column gives the peak 1400 MHz flux density, when known. --- S1400p Peak 1400 MHz flux density in Jy number=4 The integrated 1400 MHz flux is given in the S1400 column, in Jy. The u_S1400 column is marked with a colon ':' if the integrated flux is uncertain. The S1400p column gives the peak 1400 MHz flux density, when known. Jy flags Source flags number=5 This column gives flags on the source. An 'X' indicates that the source-fitting routine found an extension in RA. A 'Y' indicates a corresponding extension in declination. It is likely that in most cases such extension is caused by confusing faint sources. An evidently confused source is indicated by 'C'. Note that the X is always in the first column; the Y is always in the second column; and the C is always in the third column. Thus, a confused source has this column equal to ' C'. A question mark indicates uncertainty. --- Sp-Index Spectral index between 1400 MHz and 408 MHz number=6 The 'Sp-Index' column gives the spectral index between the 1400 MHz flux density and the 408 MHz flux density from the B2 survey, GV survey (Grueff and Vigotti 1968ApL.....2..113G), or the WK survey (Windram and Kenderdine 1969MNRAS.146..265W). A colon in the 'u_Sp-Index' column indicates a less certain spectral index. An asterisk ('*') in the u_Sp-Index column corresponds to indices given in brackets in the published paper, i.e. very uncertain spectral indices. Note that no corrections were made to the original flux density data in the other catalogs. 'Sp-Index' and 'u_Sp-Index' appear in table 'gb2.dat' only. --- u_Sp-Index ':' if spectral index is less certain number=6 The 'Sp-Index' column gives the spectral index between the 1400 MHz flux density and the 408 MHz flux density from the B2 survey, GV survey (Grueff and Vigotti 1968ApL.....2..113G), or the WK survey (Windram and Kenderdine 1969MNRAS.146..265W). A colon in the 'u_Sp-Index' column indicates a less certain spectral index. An asterisk ('*') in the u_Sp-Index column corresponds to indices given in brackets in the published paper, i.e. very uncertain spectral indices. Note that no corrections were made to the original flux density data in the other catalogs. 'Sp-Index' and 'u_Sp-Index' appear in table 'gb2.dat' only. --- Francois Ochsenbein CDS 1999 Apr 14 UNKNOWN UNKNOWN "The catalogue was originally archived as A055 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." VIII_53.xml Compendium of Radio Measurements of Bright Galaxies 8056 VIII/56 Compendium of Radio Measurements of Bright Galaxies Compendium of Radio Measurements of Bright Galaxies R F Haynes W K H Huchtmeier B Siegman A E Wright CSIRO Publication ??? ??? 1975 1975crmb.book.....H Galaxies, radio Radio sources Radio continuum This catalog contains all radio measurements of optically bright 'normal' galaxies available up until publication of this compendium in 1975. The compendium was originally intended to simplify statistical analysis of radio properties of these normal galaxies. No data processing was carried out (except to bring the data into a consistent format) and no identification was attempted. These data were originally published as Haynes, R.F., Huchtmeier, W.K.H., Siegman, Betty, and Wright, A.E., CSIRO Publication, 1975. The electronic version of this catalog has made small changes to the original version in an attempt to better identify positions with their source names. Where there was no entry on a line for the source name or position in the published version, data from the previous line was repeated.
Compendium of Radio Measurements of Bright Galaxies Name Name of source number=1 This column gives the name of the source. 'AN' refers to a designation for anonymous galaxies used by Pfleiderer (personal communication). The radio emission may sometimes originate in a region containing more than one galaxy, and in this case the designation is abbreviated, e.g. NGC4038 and NGC4039 appear as NGC4038/39. Radio components of a specific optical galaxy are indicated by a suffix, e.g. NGC4472/A, NGC4496/B and NGC3675/NUCL. In the electronic version, the "/A", "/B", etc. appear on a separate line, so it is necessary to use the name in combination with the position for a full identification. Where there was no entry in the name column of the original published table, the name from the preceding line has been repeated for ease of identification. Although in some rare cases, this may result in an incorrect identification, we felt that it was preferable to always have an identification listed, even if it is not guaranteed to be correct. --- pos_flg Position Flags number=2 This column is marked with an asterisk ('*') if the position was taken from the preceding line in the published table. Positions were repeated this way in order to guarantee that every entry had a position. A 'C' indicates that positional data was added at CDS while preparing this catalog. The information came from the name solver provided by SIMBAD. Two entries have a 'P', indicating that the identifiers found in this catalogs produced objects which were not radio Galaxies: NGC 7027 is a Planetary Nebula, NGC 2327 is an HII region, NGC 1769 is a star cluster. NGC 7072 is a galaxy though, NGC 2337 is a galaxy, NGC 1679 is also a galaxy. Despite the high chance that these were just typos, we left the positions empty for these objects. --- RAh Right Ascension (B1950) (hour) number=2 This column is marked with an asterisk ('*') if the position was taken from the preceding line in the published table. Positions were repeated this way in order to guarantee that every entry had a position. A 'C' indicates that positional data was added at CDS while preparing this catalog. The information came from the name solver provided by SIMBAD. Two entries have a 'P', indicating that the identifiers found in this catalogs produced objects which were not radio Galaxies: NGC 7027 is a Planetary Nebula, NGC 2327 is an HII region, NGC 1769 is a star cluster. NGC 7072 is a galaxy though, NGC 2337 is a galaxy, NGC 1679 is also a galaxy. Despite the high chance that these were just typos, we left the positions empty for these objects. h RAm Right Ascension (B1950) (min) number=2 This column is marked with an asterisk ('*') if the position was taken from the preceding line in the published table. Positions were repeated this way in order to guarantee that every entry had a position. A 'C' indicates that positional data was added at CDS while preparing this catalog. The information came from the name solver provided by SIMBAD. Two entries have a 'P', indicating that the identifiers found in this catalogs produced objects which were not radio Galaxies: NGC 7027 is a Planetary Nebula, NGC 2327 is an HII region, NGC 1769 is a star cluster. NGC 7072 is a galaxy though, NGC 2337 is a galaxy, NGC 1679 is also a galaxy. Despite the high chance that these were just typos, we left the positions empty for these objects. min RAs Right Ascension (B1950) (sec) number=2 This column is marked with an asterisk ('*') if the position was taken from the preceding line in the published table. Positions were repeated this way in order to guarantee that every entry had a position. A 'C' indicates that positional data was added at CDS while preparing this catalog. The information came from the name solver provided by SIMBAD. Two entries have a 'P', indicating that the identifiers found in this catalogs produced objects which were not radio Galaxies: NGC 7027 is a Planetary Nebula, NGC 2327 is an HII region, NGC 1769 is a star cluster. NGC 7072 is a galaxy though, NGC 2337 is a galaxy, NGC 1679 is also a galaxy. Despite the high chance that these were just typos, we left the positions empty for these objects. s DE- Declination sign (B1950) number=2 This column is marked with an asterisk ('*') if the position was taken from the preceding line in the published table. Positions were repeated this way in order to guarantee that every entry had a position. A 'C' indicates that positional data was added at CDS while preparing this catalog. The information came from the name solver provided by SIMBAD. Two entries have a 'P', indicating that the identifiers found in this catalogs produced objects which were not radio Galaxies: NGC 7027 is a Planetary Nebula, NGC 2327 is an HII region, NGC 1769 is a star cluster. NGC 7072 is a galaxy though, NGC 2337 is a galaxy, NGC 1679 is also a galaxy. Despite the high chance that these were just typos, we left the positions empty for these objects. --- DEd Declination (B1950) (deg) number=2 This column is marked with an asterisk ('*') if the position was taken from the preceding line in the published table. Positions were repeated this way in order to guarantee that every entry had a position. A 'C' indicates that positional data was added at CDS while preparing this catalog. The information came from the name solver provided by SIMBAD. Two entries have a 'P', indicating that the identifiers found in this catalogs produced objects which were not radio Galaxies: NGC 7027 is a Planetary Nebula, NGC 2327 is an HII region, NGC 1769 is a star cluster. NGC 7072 is a galaxy though, NGC 2337 is a galaxy, NGC 1679 is also a galaxy. Despite the high chance that these were just typos, we left the positions empty for these objects. deg DEm Declination (B1950) (arcmin) number=2 This column is marked with an asterisk ('*') if the position was taken from the preceding line in the published table. Positions were repeated this way in order to guarantee that every entry had a position. A 'C' indicates that positional data was added at CDS while preparing this catalog. The information came from the name solver provided by SIMBAD. Two entries have a 'P', indicating that the identifiers found in this catalogs produced objects which were not radio Galaxies: NGC 7027 is a Planetary Nebula, NGC 2327 is an HII region, NGC 1769 is a star cluster. NGC 7072 is a galaxy though, NGC 2337 is a galaxy, NGC 1679 is also a galaxy. Despite the high chance that these were just typos, we left the positions empty for these objects. arcmin DEs Declination (B1950) (arcsec) number=2 This column is marked with an asterisk ('*') if the position was taken from the preceding line in the published table. Positions were repeated this way in order to guarantee that every entry had a position. A 'C' indicates that positional data was added at CDS while preparing this catalog. The information came from the name solver provided by SIMBAD. Two entries have a 'P', indicating that the identifiers found in this catalogs produced objects which were not radio Galaxies: NGC 7027 is a Planetary Nebula, NGC 2327 is an HII region, NGC 1769 is a star cluster. NGC 7072 is a galaxy though, NGC 2337 is a galaxy, NGC 1679 is also a galaxy. Despite the high chance that these were just typos, we left the positions empty for these objects. arcsec l_e_RAs Denotes upper limit on ErrRA --- e_RAs Error on right ascension number=3 These columns give the errors on right ascension and declination in seconds of arc. Errors in RC2 (de Vaucouleurs and de Vaucouleurs, 1964) positions are approximately +/- 1' arc (Gallouet and Heidmann 1971A&AS....3..325G). In some cases, the error is listed as an upper limit (e.g. < 1). When the position was repeated from the preceding line, if there was an error listed, it was NOT repeated. arcsec l_e_DEs Denotes upper limit on ErrDEC --- e_DEs Error on declination number=3 These columns give the errors on right ascension and declination in seconds of arc. Errors in RC2 (de Vaucouleurs and de Vaucouleurs, 1964) positions are approximately +/- 1' arc (Gallouet and Heidmann 1971A&AS....3..325G). In some cases, the error is listed as an upper limit (e.g. < 1). When the position was repeated from the preceding line, if there was an error listed, it was NOT repeated. arcsec Freq Frequency of flux density measurement number=4 This column gives the frequency (in MHz) at which the given flux density was measured. MHz f_flux Flux density flag number=5 These columns give information about the flux density. The "f_flux" column uses the following symbols: < If the flux density is an upper limit to the radio flux for an undetected source. > If the source was extended and the given peak flux density is therefore a lower limit. ? If the flux density is questionable. C The measurement of radio emission is confused by a nearby source. --- flux Flux density in Jy number=6 The "flux" column gives the flux density of the source, in Jy. For the brightest galaxies (e.g. NGC0253), the difference between peak and integrated flux density of the source becomes appreciable. Where possible the integrated flux density is given in the table. However, the reader should refer to the original reference to ascertain which measure has been used in questionable cases. Jy e_flux Error on flux density number=7 The "e_flux" column gives the error on the flux density given in the original reference where available. Where no errors were quoted the authors have usually estimated them at approximately one-third of the flux density of the weakest detected source, thus assuming a 3 sigma detection level. Jy l_MajAxis upper or lower limit for MajAxis number=8 These columns give the angular size of the galaxy. For RC sources (de Vaucouleurs and de Vaucouleurs, 1964) the diameter is the "face-on" diameter of the optical source, in arcmin. For radio and other optical references the column gives the measured extension in right ascension and declination. Optical sizes are given either as major axis times minor axis or as a diameter "f_MajAxis = D", depending on published values (e.g. RC2 or other) and is thought to give an idea of the optical size of the galaxy to be compared with the radio beam evolved with the corresponding measurement. --- MajAxis Major axis (or diameter) number=8 These columns give the angular size of the galaxy. For RC sources (de Vaucouleurs and de Vaucouleurs, 1964) the diameter is the "face-on" diameter of the optical source, in arcmin. For radio and other optical references the column gives the measured extension in right ascension and declination. Optical sizes are given either as major axis times minor axis or as a diameter "f_MajAxis = D", depending on published values (e.g. RC2 or other) and is thought to give an idea of the optical size of the galaxy to be compared with the radio beam evolved with the corresponding measurement. arcmin f_MajAxis D indicates it is a diameter number=8 These columns give the angular size of the galaxy. For RC sources (de Vaucouleurs and de Vaucouleurs, 1964) the diameter is the "face-on" diameter of the optical source, in arcmin. For radio and other optical references the column gives the measured extension in right ascension and declination. Optical sizes are given either as major axis times minor axis or as a diameter "f_MajAxis = D", depending on published values (e.g. RC2 or other) and is thought to give an idea of the optical size of the galaxy to be compared with the radio beam evolved with the corresponding measurement. --- l_MinAxis upper or lower limit for MinAxis number=8 These columns give the angular size of the galaxy. For RC sources (de Vaucouleurs and de Vaucouleurs, 1964) the diameter is the "face-on" diameter of the optical source, in arcmin. For radio and other optical references the column gives the measured extension in right ascension and declination. Optical sizes are given either as major axis times minor axis or as a diameter "f_MajAxis = D", depending on published values (e.g. RC2 or other) and is thought to give an idea of the optical size of the galaxy to be compared with the radio beam evolved with the corresponding measurement. --- MinAxis Minor Axis number=8 These columns give the angular size of the galaxy. For RC sources (de Vaucouleurs and de Vaucouleurs, 1964) the diameter is the "face-on" diameter of the optical source, in arcmin. For radio and other optical references the column gives the measured extension in right ascension and declination. Optical sizes are given either as major axis times minor axis or as a diameter "f_MajAxis = D", depending on published values (e.g. RC2 or other) and is thought to give an idea of the optical size of the galaxy to be compared with the radio beam evolved with the corresponding measurement. arcmin type Morphological type of galaxy number=9 The optical data included in these columns are taken from RC (de Vaucouleurs and de Vaucouleurs, 1964) or from references with data which are an improvement on the RC results. Optical data are not included for those sources for which only upper limits to the radio flux density are known. The "type" column gives the morphological type of the galaxy as given in the listed references. Generally, a simplified Hubble classification has been used. The "B-V" and "U-B" columns give the B-V and U-B colors which are taken from RC. The apparent photographic magnitude is given in the "Pmag" column (B(0) or m(c) or m(H) in decreasing order of preference). The total corrected apparent magnitude is given in the "Btc" column, obtained from the B(0) magnitude given in RC or, where B(0) is not available, from m(c) or m(H). The magnitude thus obtained was corrected for galactic and internal absorption and then extrapolated to a total magnitude using the method of Cameron (1971). Data provided by R.R. Shobbrook (personal communication) were also used. The "Rvel" column gives the radial velocity (in km/s) of the galaxy relative to the galactic standard of rest. The circular velocity of the Sun is taken to be 250 km/s. --- B-V B-V color index number=9 The optical data included in these columns are taken from RC (de Vaucouleurs and de Vaucouleurs, 1964) or from references with data which are an improvement on the RC results. Optical data are not included for those sources for which only upper limits to the radio flux density are known. The "type" column gives the morphological type of the galaxy as given in the listed references. Generally, a simplified Hubble classification has been used. The "B-V" and "U-B" columns give the B-V and U-B colors which are taken from RC. The apparent photographic magnitude is given in the "Pmag" column (B(0) or m(c) or m(H) in decreasing order of preference). The total corrected apparent magnitude is given in the "Btc" column, obtained from the B(0) magnitude given in RC or, where B(0) is not available, from m(c) or m(H). The magnitude thus obtained was corrected for galactic and internal absorption and then extrapolated to a total magnitude using the method of Cameron (1971). Data provided by R.R. Shobbrook (personal communication) were also used. The "Rvel" column gives the radial velocity (in km/s) of the galaxy relative to the galactic standard of rest. The circular velocity of the Sun is taken to be 250 km/s. mag U-B U-B color index number=9 The optical data included in these columns are taken from RC (de Vaucouleurs and de Vaucouleurs, 1964) or from references with data which are an improvement on the RC results. Optical data are not included for those sources for which only upper limits to the radio flux density are known. The "type" column gives the morphological type of the galaxy as given in the listed references. Generally, a simplified Hubble classification has been used. The "B-V" and "U-B" columns give the B-V and U-B colors which are taken from RC. The apparent photographic magnitude is given in the "Pmag" column (B(0) or m(c) or m(H) in decreasing order of preference). The total corrected apparent magnitude is given in the "Btc" column, obtained from the B(0) magnitude given in RC or, where B(0) is not available, from m(c) or m(H). The magnitude thus obtained was corrected for galactic and internal absorption and then extrapolated to a total magnitude using the method of Cameron (1971). Data provided by R.R. Shobbrook (personal communication) were also used. The "Rvel" column gives the radial velocity (in km/s) of the galaxy relative to the galactic standard of rest. The circular velocity of the Sun is taken to be 250 km/s. mag Pmag Apparent photographic magnitude number=9 The optical data included in these columns are taken from RC (de Vaucouleurs and de Vaucouleurs, 1964) or from references with data which are an improvement on the RC results. Optical data are not included for those sources for which only upper limits to the radio flux density are known. The "type" column gives the morphological type of the galaxy as given in the listed references. Generally, a simplified Hubble classification has been used. The "B-V" and "U-B" columns give the B-V and U-B colors which are taken from RC. The apparent photographic magnitude is given in the "Pmag" column (B(0) or m(c) or m(H) in decreasing order of preference). The total corrected apparent magnitude is given in the "Btc" column, obtained from the B(0) magnitude given in RC or, where B(0) is not available, from m(c) or m(H). The magnitude thus obtained was corrected for galactic and internal absorption and then extrapolated to a total magnitude using the method of Cameron (1971). Data provided by R.R. Shobbrook (personal communication) were also used. The "Rvel" column gives the radial velocity (in km/s) of the galaxy relative to the galactic standard of rest. The circular velocity of the Sun is taken to be 250 km/s. mag f_Pmag Notes on Pmag number=9 The optical data included in these columns are taken from RC (de Vaucouleurs and de Vaucouleurs, 1964) or from references with data which are an improvement on the RC results. Optical data are not included for those sources for which only upper limits to the radio flux density are known. The "type" column gives the morphological type of the galaxy as given in the listed references. Generally, a simplified Hubble classification has been used. The "B-V" and "U-B" columns give the B-V and U-B colors which are taken from RC. The apparent photographic magnitude is given in the "Pmag" column (B(0) or m(c) or m(H) in decreasing order of preference). The total corrected apparent magnitude is given in the "Btc" column, obtained from the B(0) magnitude given in RC or, where B(0) is not available, from m(c) or m(H). The magnitude thus obtained was corrected for galactic and internal absorption and then extrapolated to a total magnitude using the method of Cameron (1971). Data provided by R.R. Shobbrook (personal communication) were also used. The "Rvel" column gives the radial velocity (in km/s) of the galaxy relative to the galactic standard of rest. The circular velocity of the Sun is taken to be 250 km/s. --- Btc Total corrected apparent magnitude number=9 The optical data included in these columns are taken from RC (de Vaucouleurs and de Vaucouleurs, 1964) or from references with data which are an improvement on the RC results. Optical data are not included for those sources for which only upper limits to the radio flux density are known. The "type" column gives the morphological type of the galaxy as given in the listed references. Generally, a simplified Hubble classification has been used. The "B-V" and "U-B" columns give the B-V and U-B colors which are taken from RC. The apparent photographic magnitude is given in the "Pmag" column (B(0) or m(c) or m(H) in decreasing order of preference). The total corrected apparent magnitude is given in the "Btc" column, obtained from the B(0) magnitude given in RC or, where B(0) is not available, from m(c) or m(H). The magnitude thus obtained was corrected for galactic and internal absorption and then extrapolated to a total magnitude using the method of Cameron (1971). Data provided by R.R. Shobbrook (personal communication) were also used. The "Rvel" column gives the radial velocity (in km/s) of the galaxy relative to the galactic standard of rest. The circular velocity of the Sun is taken to be 250 km/s. mag Rvel Radial velocity of the galaxy number=9 The optical data included in these columns are taken from RC (de Vaucouleurs and de Vaucouleurs, 1964) or from references with data which are an improvement on the RC results. Optical data are not included for those sources for which only upper limits to the radio flux density are known. The "type" column gives the morphological type of the galaxy as given in the listed references. Generally, a simplified Hubble classification has been used. The "B-V" and "U-B" columns give the B-V and U-B colors which are taken from RC. The apparent photographic magnitude is given in the "Pmag" column (B(0) or m(c) or m(H) in decreasing order of preference). The total corrected apparent magnitude is given in the "Btc" column, obtained from the B(0) magnitude given in RC or, where B(0) is not available, from m(c) or m(H). The magnitude thus obtained was corrected for galactic and internal absorption and then extrapolated to a total magnitude using the method of Cameron (1971). Data provided by R.R. Shobbrook (personal communication) were also used. The "Rvel" column gives the radial velocity (in km/s) of the galaxy relative to the galactic standard of rest. The circular velocity of the Sun is taken to be 250 km/s. km/s r_Opt Comma-separated references for optical data (see file refs.dat) --- r_Rad Reference for radio data (see file refs.dat) --- References code reference code, repeated when several lines are required. --- ref_text Bibcode (if available) and reference text --- Patricio Ortiz, Francois Ochsenbein CDS 1999 Apr 23 UNKNOWN UNKNOWN * Prepared by H.Andernach, Feb. 1992: The Compendium of radio observations of normal galaxies was received in April 1991 from W.Huchtmeier on diskette. The following corrections were applied: - a column shift for IC1559 by one column to right - all blank lines (N=1864) and those containing the string 'CONTINUED' (N=125) were deleted - morphological types were coded in the original file in only upper case letters in the "type" column. They were transformed to the types as published with a special routine and inserted properly for the '---' strings of the original file (213 cases) * Made available as table "rad_br_gals" at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) by Carloyn Stern. VIII_56.xml Fluxes of Faint Radio Sources at 2.7/4.75 GHz (32.8d--33.5{deg}) 8057 VIII/57 Fluxes of Faint Radio Sources at 2.7/4.75 GHz Fluxes of Faint Radio Sources at 2.7/4.75 GHz (32.8d--33.5{deg}) T Forkert D R Altschuler Astron. Astrophys. Suppl. Ser. 70 77 1987 1987A&AS...70...77F Radio continuum Radio sources This table is a compilation of revised 4.75 GHz and 2.695 GHz flux densities and corresponding spectral indices at epoch 1986.2 of a catalog of 239 sources, which has previously been published by Forkert and Altschuler, (1987A&AS...70...77F). It comprises 209 sources (marked 'A'), forming a complete, flux density limited sample above 50 mJy at 4.76 GHz in 1981.9 (Altschuler, 1986A&AS...65..267A), and 30 sources (marked 'a') below this limit, but with 5.0 GHz flux densities from 1971.0 (Davis, 1971AJ.....76..980D). The catalogue covers a narrow strip of the sky around declination of 33 degrees. The flux densities were calibrated with 3C286 on the scale of Kellermann, Pauliny-Toth and Williams (1969ApJ...157....1K). After publication of the catalog a statistical analysis for flux density variability in the data has been performed (Forkert, 1990), using 6cm flux density measurements of Davis (1971AJ.....76..980D) and Altschuler (1986A&AS...65..267A) and the 2.695 GHz flux densities of Pauliny-Toth et al. (1974A&A....35..421P), the details and results of which are going to be published elsewhere (Altschuler & Forkert, in preparation). For the purposes of this analysis it has become necessary to obtain more individual error estimates of the 1986.2 data, not dominated by the effect of overall scale errors. This revision for some of the sources also led to slightly different flux densities from those previously published. The variability study proved the flux density errors to represent the individual 1-sigma uncertainties, WITHOUT the effect of overall scale errors. From the aforementioned comparison with other measurements scale errors of ~1% at 2.695 GHz and ~3% at 4.75 GHz seem likely.
Fluxes of Faint Radio Sources at 2.7/4.75 GHz (32.8{deg} < Dec < 33.5{deg}) Seqno Sequence number of source number=1 These columns give the sequence number and the name of the source. The number is assigned sequentially in right ascension to all sources in the catalog. The name is assigned using IAU conventions, as hhmm+ddmm, with a letter appended at the end if necessary to determine uniqueness. --- Name IAU name of source number=1 These columns give the sequence number and the name of the source. The number is assigned sequentially in right ascension to all sources in the catalog. The name is assigned using IAU conventions, as hhmm+ddmm, with a letter appended at the end if necessary to determine uniqueness. --- RAh Right Ascension (B1950) (hour) number=2 These columns contain the B1950 coordinates of the source, in radians and in degrees. The sources were observed at the 5 GHz positions determined by Altschuler (1986A&AS...65..267A). Positional errors at 5 GHz are given in that paper. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=2 These columns contain the B1950 coordinates of the source, in radians and in degrees. The sources were observed at the 5 GHz positions determined by Altschuler (1986A&AS...65..267A). Positional errors at 5 GHz are given in that paper. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec S2695 Peak flux density of source at 2695 MHz mJy e_S2695 Error on 2695 flux density mJy S4750 Peak flux density of source at 4750 MHz mJy e_S4750 Error on 4750 flux density mJy Sp+Index Spectral index between 2.7 and 4.75 GHz number=3 These columns give the spectral index and error. The spectral index was computed as: alpha = 1.77 * ln [S_2.7_/S_4.75_] ( S_{nu}_ {prop.to} {nu}^{alpha}^ ) and its error as: e_alpha = 1.77 * sqrt [ (sigma_tot/S_4.75_)^2^ + (sigma_tot/S_2.7_)^2^ ] where sigma_tot was estimated from measurements of individual scans and is typically 3 mJy (see the paper for details). --- e_Sp+Index Error on spectral index number=3 These columns give the spectral index and error. The spectral index was computed as: alpha = 1.77 * ln [S_2.7_/S_4.75_] ( S_{nu}_ {prop.to} {nu}^{alpha}^ ) and its error as: e_alpha = 1.77 * sqrt [ (sigma_tot/S_4.75_)^2^ + (sigma_tot/S_2.7_)^2^ ] where sigma_tot was estimated from measurements of individual scans and is typically 3 mJy (see the paper for details). --- Oname Other name of source --- comment Comments on source number=4 This column gives comments on the source as follows: a, A - Source below or above the completeness limit of 50mJy in the survey at 4.76GHz in 1981.9 of Altschuler, Altschuler (1986A&AS...65..267A). d, D - Source below or above the completeness limit of 67mJy in the survey at 5.0GHz in 1971.0 of Davis, Davis (1971AJ.....76..980D) c_x - Confusing components were present at x cm wavelength and have been subtracted e?_x - Possibly extended at x cm wavelength --- Patricio Ortiz CDS 1999 Apr 23 UNKNOWN UNKNOWN The data were provided by T. Forkert to H. Andernach in late 1990, who provided them to ADS/Einline (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) VIII_57.xml A Survey of Radio H II Regions in the Northern Sky 8058 VIII/58 A Survey of Radio H II Regions in the Northern Sky A Survey of Radio H II Regions in the Northern Sky F J Lockman Astrophys. J. Suppl. 71 469 1989 1989ApJS...71..469L H II regions Radio sources Radio lines Surveys Nearly 500 radio continuum sources near the Galactic plane at declinations greater than -37 degrees were examined for radio recombination line emission to see if they might be HII regions. A total of 462 were detected, about half of these for the first time. The data are presented in an extensive table. Among the newly discovered nebulae are several with recombinations lines so narrow that their electron temperature must be less than 4600 K. In one case the line width (in several transitions) is only 11.6 km/s, requiring electron temperatures less than about 2900 K.
Catalog of radio H II regions GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right Ascension (1950) h RAm Right Ascension (1950) min RAs Right Ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec T Peak antenna temperature of detected line mK e_T Uncertainty (1 sigma) in peak antenna temperature mK FWHM Full-width at half-maximum of detected line km/s e_FWHM Uncertainty (1 sigma) in FWHM km/s VLSR Velocity with respect to the local standard of rest km/s e_VLSR Uncertainty (1 sigma) in VLSR km/s GRMS RMS deviation of observed line from Gaussian fit mK BRMS RMS in baseline parts of spectrum mK Notes Source Comments Mainly gives name of optical counterpart to radio source. Also identifies sources observed at bands other than or in addition to 3 cm. If an H II region has been detected in several bands, the most accurate measurement is listed and the others just noted. Letter "D" refers to sources that show two recombination lines at distinctly different velocities. "Note" indicates that there are additonal notes in main reference. --- Tom Sodroski SSDOO/ADC 1999 Jul 26 H. Andernach <Heinz.Andernach@astro.ugto.mx> and S. Trushkin scanned the published data table, made format changes, and provided a copy of their electronic version to ADC. VIII_58.xml The ROSAT all-sky survey bright source catalogue. 9010A IX/10A ROSAT All-Sky Bright Source Catalogue The ROSAT all-sky survey bright source catalogue. W Voges B Aschenbach T Boller H Braeuninger U Briel W Burkert K Dennerl J Englhauser R Gruber F Haberl G Hartner G Hasinger M Kuerster E Pfeffermann W Pietsch P Predehl C Rosso J H M M Schmitt J Truemper H U Zimmermann Astron. Astrophys. 349 389 1999 1999A&A...349..389V IX/11 : the ROSAT Source Catalogue (Voges+ 1995) IX/12 : the WGACAT version of the ROSAT PSPC Catalogue (White+ 1995) IX/28 : ROSAT HRI Pointed Observations (1RXH) (ROSAT Team, 1999) J/A+AS/114/465 : ROSAT XUV Pointed Phase Source Catalogue (Kreysing+ 1995) J/MNRAS/274/1165 : The 2RE Source Catalogue (Pye+ 1995) http://www.rosat.mpe-garching.mpg.de/survey/rass-bsc : the WWW page X-ray sources catalogs surveys X-rays: general The ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, revision 1RXS) is derived from the all-sky survey performed during the first half year (1990/91) of the ROSAT mission. 18,806 sources are catalogued (five sources were removed compared to the 18,811 sources of the 1996 version), down to a limiting ROSAT PSPC count-rate of 0.05cts/s in the 0.1-2.4keV energy band, with a detection likelihood of at least 15 and with at least 15 source photons. For 94% of the sources visual inspection confirmed the results of the standard processing with respect to existence and position; the remaining 6% were re-analysed and appropriately flagged. At a brightness limit of 0.1cts/s (8,547 sources) the catalogue represents a sky coverage of 92%. Broad band images are available for a subset of the flagged sources from http://wave.xray.mpe.mpg.de/rosat/catalogues/rass-bsc . Questions or comments may be directed to <survey@rosat.mpe-garching.mpg.de>
ROSAT
The 1RXS catalogue 1RXS ROSAT All-Sky Survey Catalogue source name number=1 The name includes the '1RXS' acronym, and is based on J2000 position (format JHHMMSS.S+DDMMSS). This name is used in the generation of a link to a broad band image if this image is available (see NewFlag, and Note (3)) See the changes in sources compared to the 1996 version in the "History" section below --- n_1RXS Names modified from previous version --- RAdeg Right ascension (J2000), decimal degrees deg DEdeg Declination (J2000), decimal degrees deg PosErr Total positional error (including 6" systematic error) arcsec ScrFlags screening flags number=2 the flags are 'T' for 'true', 'F' or '_' for 'false'; '.' for not used n (byte 48) nearby sources affecting SASS flux determination p (byte 49) possible problem with position determination e (byte 50) source extended beyond SASS extraction radius d (byte 51) complex diffuse emission pattern m (byte 52) source missed by SASS --- NewFlag 'new data' flags number=3 the flags are 'T' for 'true', 'F' or '_' for 'false'; '.' for not used r (byte 54) source counts and extraction radius recalculated i (byte 55) broad band image available (html link!) v (byte 56) variability flag (not yet filled) . (byte 57) dummy flag --- Count Source countrate number=4 Countrates are vignetting corrected ct/s e_Count Error on Count number=4 Countrates are vignetting corrected ct/s bgCt Background countrate number=4 Countrates are vignetting corrected ct/s/arcmin2 ExpTime Exposure time s HR1 Hardness ratio 1 number=5 The hardness ratios are defined by: hr1 = ( B - A ) / ( B + A ) , where A = countrate in PHA range 11 - 41 (~ 0.1-0.4 keV) B = countrate in PHA range 52 - 201 (~ 0.5-2.0 keV) hr2 = ( D - C ) / ( D + C ) , where C = countrate in PHA range 52 - 90 (~ 0.5-0.9 keV) D = countrate in PHA range 91 - 201 (~ 0.9-2.0 keV) (PHA = Pulse Height Amplitude) --- e_HR1 Error on HR1 number=6 the true mean error is probably bigger, and values larger than 9.99 are set to 9.99 --- HR2 hardness ratio 2 number=5 The hardness ratios are defined by: hr1 = ( B - A ) / ( B + A ) , where A = countrate in PHA range 11 - 41 (~ 0.1-0.4 keV) B = countrate in PHA range 52 - 201 (~ 0.5-2.0 keV) hr2 = ( D - C ) / ( D + C ) , where C = countrate in PHA range 52 - 90 (~ 0.5-0.9 keV) D = countrate in PHA range 91 - 201 (~ 0.9-2.0 keV) (PHA = Pulse Height Amplitude) --- e_HR2 Error on HR2 number=6 the true mean error is probably bigger, and values larger than 9.99 are set to 9.99 --- Extent Source extent, by which the source image exceeds the point spread function. arcsec L_Extent Likelihood of source extent number=7 values larger than 9999 are set to 9999 --- Ldetect Likelihood of source detection algorithm number=7 values larger than 9999 are set to 9999 --- ExtRad Extraction radius arcsec PrioFlags priority flags number=8 the flags indicate the sliding window detection history using either the background map (M) or the local background (B), and take the values 0 = no detection, 1 = detection; The order of flags is: M-broad, L-broad, M-hard, L-hard, M-soft, L-soft --- PHA PHA range of best detection number=9 the PHA (Pulse Height Amplitude) range PHA range with highest detection likelihood is indicated by A = PHA range 11-41 (~ 0.1-0.4 keV) B = PHA range 52-201 (~ 0.5-2.0 keV) C = PHA range 52-90 (~ 0.5-0.9 keV) D = PHA range 91-201 (~ 0.9-2.0 keV) b or blank means 'broad' --- VigFactor Vignetting factor --- IncDate Date when source was included number=10 a value "000000" for the date indicates a removed source "YYMMDD" UpdDate Date when source properties changed number=11 a value "000000" indicates not-applicable date "YYMMDD" Ncand Number of identification candidates in the correlation catalogue --- SASS Identification number of SASS field number=12 An overview of the field structure is available at URL <http://www.rosat.mpe-garching.mpg.de/survey/rass-bsc/sup/psplit.ps.gz> --- --- --- MASOL SASS source number (MASOL number) in SASS field (mainly for internal use) --- 1RXS Correlation entries 1RXS 1RXS name --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg PosErr Total positional error arcsec Nid Number of correlated sources --- --- Name of source catalogue (always 1RXS) --- bandPos origin of the source position (always x: X-ray) --- gal_Nh Galactic HI column density (in 10^21^atoms/cm^2^) 10+21cm-2 GLON Galactic longitude deg GLAT Galactic latitude deg HR1 Hardness ration 1 --- e_HR1 rms uncertainty on HR1 --- HR2 Hardness ration 2 --- e_HR2 rms uncertainty on HR2 --- Extent Source extent --- L_Extent Likelihood of source extent --- Ldetect Likelihood of source detection algorithm --- ExpTime Exposure time s Count Source count rate ct/s e_Count rms uncertainty on Count ct/s Flux1 X-ray flux 1 in 0.1-2.4keV energy range mW/m2 Flux2 X-ray flux 2 in 0.1-2.4keV energy range mW/m2 begDate First date of observation "YYMMDD" begDate.f First date of observation (day fraction) d endDate Last date of observation "YYMMDD" endDate.f Last date of observation (day fraction) d IncDate Date when source was included "YYMMDD" UpdDate Date when source properties changed "YYMMDD" 1RXS Correlation to IRASPSC, IRASFSC 1RXS 1RXS source name --- Rank Rank in correlation list for the source --- sourceID Source identification number=1 the IRASPSC numbers do not correspond to the usual IRAS designations. --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Sep Separation arcsec PA Position angle deg r_sourceID Source catalogue (see file "refs.dat") --- bandPos Origin of the source position (i: IR) --- Type Type or class of object --- F12mu Infrared flux in the 12{mu}m band Jy F25mu Infrared flux in the 25{mu}m band Jy F60mu Infrared flux in the 60{mu}m band Jy F100mu Infrared flux in the 100{mu}m band Jy Com Comments --- IncDate Date when source was included "YYMMDD" UpdDate Date when source properties were changed "YYMMDD" 1RXS Correlation to NED 1RXS 1RXS source name --- Rank Rank in correlation list for the source --- sourceID Source identification --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Sep Separation arcsec PA Position angle deg r_sourceID Source catalogue (see file "refs.dat") --- bandPos Origin of the source position number=1 o: optical; x: X-ray; r: Radio; e: EUV; i: IR --- Type Type or class of object --- fxfopt Ratio of X-ray to optical flux f_X / f_opt --- l_vmag Limit flag on vmag --- vmag Visual magnitude mag n_vmag : => Uncertainty flag on vmag / => interval of magnitude + => 18+ ??? --- vmag2 Second value of vmag when interval --- u_vmag2 Uncertainty flag on vmag2 --- z Redshift --- l_NED-flux Limit flag on NED-flux --- NED-flux Radio flux density or IR flux density in the band given in fl-band mJy fl-band Frequency band or wavelength band used for flux given in NED-flux (Radio [GHz], IR [mJy] for NED) mum l_Size Limit flag on Size --- Size Size of object arcmin u_Size Uncertainty flag on Size --- Com Comments --- IncDate Date when source was included "YYMMDD" UpdDate Date when source properties were changed "YYMMDD" 1RXS Correlation to NVSS, FIRST 1RXS 1RXS source name --- Rank Rank in correlation list for the source --- sourceID Source identification --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Sep Separation arcsec PA Position angle deg r_sourceID Source catalogue (see file "refs.dat") --- bandPos Origin of the source position number=1 o: optical; x: X-ray; r: Radio; e: EUV; i: IR --- Type Type or class of object --- dist Distance kpc F20cm(I) Radio integrated flux density in the 20cm band mJy F20cm(P) Radio peak flux density in the 20cm band mJy IncDate Date when source was included "YYMMDD" UpdDate Date when source properties were changed "YYMMDD" 1RXS Correlation to HST_GSC 1RXS Correlation to PRI, RITTER, SIMBAD, TYCHO, EUVE 1RXS Correlation to ROSAT-WFC 1RXS 1RXS source name --- Rank Rank in correlation list for the source --- sourceID Source identification (see also r_sourceID) --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Sep Separation arcsec PA Position angle deg r_sourceID Source catalogue (see file "refs.dat") --- bandPos Origin of the source position number=1 o: optical; x: X-ray; r: Radio; e: EUV; i: IR --- Type Type or class of object --- fxfopt Ratio of X-ray to optical flux f_X / f_opt --- l_vmag Limit flag on vmag --- vmag Visual magnitude mag bmag Blue magnitude mag rmag Red magnitude mag b-r (blue-red) colour mag b-v (blue-visual) colour mag u-b (ultraviolet-blue) colour mag var Variability flag --- n_z Note on z --- z Redshift (from PRI or SIMBAD) --- Vr Radial velocity (from SIMBAD only) km/s dist Distance kpc Com Comments --- IncDate Date when source was included "YYMMDD" UpdDate Date when source properties were changed "YYMMDD" 1RXS Correlation to ROSATP3, ROSATWGA, ROSATHRI 1RXS 1RXS source name --- Rank Rank in correlation list for the source --- sourceID Source identification --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Sep Separation arcsec PA Position angle deg r_sourceID Source catalogue (see file "refs.dat") --- bandPos Origin of the source position number=1 o: optical; x: X-ray; r: Radio; e: EUV; i: IR --- Type Type or class of object --- HR1 Hardness ration 1 --- e_HR1 rms uncertainty on HR1 --- HR2 Hardness ration 2 --- e_HR2 rms uncertainty on HR2 --- Extent Source extent --- L_Extent Likelihood of source extent --- Ldetect Likelihood of source detection algorithm --- ExpTime Exposure time s Count Source countrate --- e_Count rms uncertainty on Count --- roff Off-axis angle arcmin Com Comments --- IncDate Date when source was included "YYMMDD" UpdDate Date when source properties were changed "YYMMDD" 1RXS Correlation Catalogue to VERRON8 1RXS 1RXS source name --- Rank Rank in correlation list for the source --- sourceID Source identification --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Sep Separation arcsec PA Position angle deg r_sourceID Source catalogue (see file "refs.dat") --- bandPos Origin of the source position number=1 o: optical; x: X-ray; r: Radio; e: EUV; i: IR --- Type Type or class of object --- fxfopt Ratio of X-ray to optical flux f_X / f_opt --- l_vmag Limit flag on vmag --- vmag Visual magnitude mag rmag Red magnitude mag b-v (blue-visual) colour mag u-b (ultraviolet-blue) colour mag n_z Note on z --- z Redshift --- R-f6cm R-f6cm in the 6cm band mJy R-f11cm R-f11cm in the 11cm band mJy Com Comments --- IncDate Date when source was included "YYMMDD" UpdDate Date when source properties were changed "YYMMDD" References catal-id Name of source catalogue --- Aut Author names --- BibCode BibCode --- Com Comments --- 1rxscorr.txt The ROSAT All-Sky Survey Bright Source Correlation Catalogue in a single file fields.ps Plot describing the field structure (postscript) screen.ps Details about screening methods (postscript) Francois Ochsenbein, Patricia Bauer CDS 1999 Nov 05 UNKNOWN UNKNOWN * 15-Jul-1996 (Catalog IX/10): The catalog (Version 14-Jun-1996) was copied via FTP from ftp://ftp.rosat.mpe-garching.mpg.de/archive/survey/rass-bsc * 11-Oct-1999 (Catalog IX/10A): The catalog (Version 10-Jun-1999) was copied via FTP from ftp://ftp.xray.mpe.mpg.de/rosat/catalogues/rass-bsc Compared to the 14-Jun-1996 version: => five sources were removed: 1RXS J050251.5-622744 1RXS J054919.1-620511 1RXS J055054.2-621454 1RXS J055225.0-640206 1RXS J055529.5-640618 => 14 sources were renamed: 1RXS J050531.2-614456 renamed 1RXS J050531.3-614456 1RXS J050644.7-610943 renamed 1RXS J050644.8-610943 1RXS J051545.5-643812 renamed 1RXS J051545.6-643812 1RXS J051615.8-631319 renamed 1RXS J051615.9-631319 1RXS J051934.0-604800 renamed 1RXS J051934.1-604800 1RXS J052124.2-641851 renamed 1RXS J052124.3-641851 1RXS J052630.7-602227 renamed 1RXS J052630.8-602227 1RXS J052641.0-623959 renamed 1RXS J052641.1-623959 1RXS J053431.8-601613 renamed 1RXS J053431.9-601613 1RXS J053855.5-640457 renamed 1RXS J053855.6-640457 1RXS J054053.0-614312 renamed 1RXS J054053.1-614312 1RXS J054236.0-615414 renamed 1RXS J054236.1-615414 1RXS J054513.1-595527 renamed 1RXS J054513.2-595527 1RXS J181545.4+164043 renamed 1RXS J181545.4-164043 IX_10A.xml The ROSAT All-Sky Bright Source Catalogue 9010 IX/10 ROSAT All-Sky Bright Source Catalogue The ROSAT All-Sky Bright Source Catalogue W Voges B Aschenbach Th Boller H Braeuninger U G Briel W Burkert K Dennerl J Englhauser R Gruber F Haberl G Hartner G Hasinger M Kuerster E Pfeffermann W Pietsch P Predehl C Rosso J H M M Schmitt J Truemper H -U Zimmermann IAU Circ. 6420 2 1996 1996IAUC.6420....2V IX/11 : the ROSAT Source Catalogue (Voges+ 1995) IX/12 : the WGACAT version of the ROSAT PSPC Catalogue (White+ 1995) J/A+AS/114/465 : ROSAT XUV Pointed Phase Source Catalogue (Kreysing+ 1995) J/MNRAS/274/1165 : The 2RE Source Catalogue (Pye+ 1995) http://www.rosat.mpe-garching.mpg.de/survey/rass-bsc : the WWW page X-ray sources The ROSAT ALL-SKY SURVEY BRIGHT SOURCE CATALOGUE (RASS-BSC, revision 1RXS) is derived from the all-sky survey performed during the first half year of the ROSAT mission in 1990/91. 18,811 sources are catalogued, with a limiting ROSAT PSPC countrate of 0.05 cts/s in the 0.1-2.4 keV energy band. The sources have a detection likelihood of at least 15 and contain at least 15 source photons. At a brightness limit of 0.1 cts/s (8,547 sources) the catalogue represents a sky coverage of 92%. For each source the ROSAT name, the position in equatorial co-ordinates, the positional error, the source countrate and error, the background countrate, exposure time, hardness-ratios HR1 and HR2 and errors, extent and likelihood of extent, and likelihood of detection are provided. For 94% of the sources visual inspection confirmed the results of the standard processing with respect to existence and position; the remaining 6% were re-analysed and appropriately flagged. Broad band images are available for a subset of the flagged sources. Questions or comments may be directed to <survey@rosat.mpe-garching.mpg.de>
ROSAT
The 1RXS catalogue Name ROSAT All-Sky Survey Catalogue source name number=1 The name includes the '1RXS' acronym, and is based on J2000 position (format JHHMMSS.S+DDMMSS). This name is used in the generation of a link to a broad band image if this image is available (see NewFlag, and Note (3)) --- RAdeg Right ascension (J2000), decimal degrees deg DEdeg Declination (J2000), decimal degrees deg PosErr Total positional error (including 6" systematic error) arcsec ScrFlags screening flags number=2 the flags are '-' for false, '.' for not used, and: n (byte 48) nearby sources affecting SASS flux determination p (byte 49) possible problem with position determination e (byte 50) source extended beyond SASS extraction radius d (byte 51) complex diffuse emission pattern m (byte 52) source missed by SASS --- NewFlag 'new data' flags number=3 the flags are '-' for false, '.' for dummy or not used, and: r (byte 54) source counts and extraction radius recalculated i (byte 55) broad band image available (html link!) v (byte 56) variability flag (not yet filled) --- Count Source countrate number=4 Counrtates are vignetting corrected ct/s e_Count Error on Count number=4 Counrtates are vignetting corrected ct/s bgCt Background countrate number=4 Counrtates are vignetting corrected ct/s/arcmin2 ExpTime Exposure time s HR1 Hardness ratio 1 number=5 The hardness ratios are defined by: hr1 = ( B - A ) / ( B + A ) , where A = countrate in PHA range 11 - 41 (~ 0.1-0.4 keV) B = countrate in PHA range 52 - 201 (~ 0.5-2.0 keV) hr2 = ( D - C ) / ( D + C ) , where C = countrate in PHA range 52 - 90 (~ 0.5-0.9 keV) D = countrate in PHA range 91 - 201 (~ 0.9-2.0 keV) (PHA = Pulse Height Amplitude) --- e_HR1 Error on HR1 number=6 the true mean error is probably bigger, and values larger than 9.99 are set to 9.99 --- HR2 hardness ratio 2 number=5 The hardness ratios are defined by: hr1 = ( B - A ) / ( B + A ) , where A = countrate in PHA range 11 - 41 (~ 0.1-0.4 keV) B = countrate in PHA range 52 - 201 (~ 0.5-2.0 keV) hr2 = ( D - C ) / ( D + C ) , where C = countrate in PHA range 52 - 90 (~ 0.5-0.9 keV) D = countrate in PHA range 91 - 201 (~ 0.9-2.0 keV) (PHA = Pulse Height Amplitude) --- e_HR2 Error on HR2 number=6 the true mean error is probably bigger, and values larger than 9.99 are set to 9.99 --- Extent Source extent, by which the source image exceeds the point spread function. arcsec L_Extent Likelihood of source extent number=7 values larger than 9999 are set to 9999 --- Ldetect Likelihood of source detection algorithm number=7 values larger than 9999 are set to 9999 --- ExtRad Extraction radius arcsec PrioFlags priority flags number=8 the flags indicate the sliding window detection history using either the background map (M) or the local background (B), and take the values 0 = no detection, 1 = detection; The order of flags is: M-broad, L-broad, M-hard, L-hard, M-soft, L-soft --- PHA PHA range of best detection number=9 the PHA (Pulse Height Amplitude) range PHA range with highest detection likelihood is indicated by A = PHA range 11-41 (~ 0.1-0.4 keV) B = PHA range 52-201 (~ 0.5-2.0 keV) C = PHA range 52-90 (~ 0.5-0.9 keV) D = PHA range 91-201 (~ 0.9-2.0 keV) b or blank means 'broad' --- VigFactor Vignetting factor --- IncDate Date when source was included number=10 a value "000000" for the date indicates a removed source "YYMMDD" UpdDate date when source properties were changed number=11 a value "000000" indicates not-applicable date "YYMMDD" --- dummy column --- SASS Identification number of SASS field number=12 An overview of the field structure is available at URL <http://www.rosat.mpe-garching.mpg.de/survey/rass-bsc/sup/psplit.ps.gz> --- --- --- MASOL SASS source number (MASOL number) in SASS field (mainly for internal use) --- fields.ps Plot describing the field structure(postscript) screening.ps Details about screening methods (postscript) CDS Catalogues Service CDS 1996 Jul 15 UNKNOWN UNKNOWN The catalog (Version 14-Jun-1996) was copied via FTP from ftp://ftp.rosat.mpe-garching.mpg.de/archive/survey/rass-bsc IX_10.xml ROSAT Source Catalog, Version 11-May-1995 9011 IX/11 ROSAT Source Catalog ROSAT Source Catalog, Version 11-May-1995 W Voges R Gruber F Haberl M Kuerster W Pietsch U Zimmermann ROSAT NEWS No.32 ??? ??? 01-Nov-1994 1994 IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) IX/12 : the WGACAT version of the ROSAT PSPC Catalogue (White+ 1995) J/A+AS/114/465 : ROSAT XUV Pointed Phase Source Catalogue (Kreysing+ 1995) J/MNRAS/274/1165 : The 2RE Source Catalogue (Pye+ 1995) http://www.rosat.mpe-garching.mpg.de/RDA : Public ROSAT Data ArchiveTruemper J., 1983, Adv. in Space Res. 2, No.4, 241. X-ray sources This catalogue contains sources from PSPC-ROSAT (Position-sensitive Proportional Counter aboard the Roentgen Satellite), as provided by Max-Planck Institut fuer extraterrestrische Physik (MPE) in December 1994. The WGACAT version of the ROSAT PSPC Catalogue (IX/12) is a similar catalogue with slightly different reduction procedures For a description of the ROSAT Mission, see Truemper (1983)
ROSAT
The ROSAT Source Catalogue Seq ROSAT observation sequence number --- MASOL MASOL main running number --- Name ROSAT source name (1RXP) number=1 The name includes the '1RXP' acronym, and is based on J2000 position (format JHHMMSS.S+DDMMSS). --- RAdeg Right ascension (J2000), decimal degrees deg DEdeg Declination (J2000), decimal degrees deg GLON Galactic longitude deg GLAT Galactic latitude deg ErrML Positional accuracy: error radius of Maximum Likelihood algorithm arcsec ErrBor Positional accuracy: boresight error arcsec ErrSys Positional accuracy: systematic error arcsec PosErr Total Positional accuracy arcsec OffAxis Off-axis radius in arcmin arcmin Count Source countrate (vignetting corrected) ct/s e_Count Mean error on Count ct/s bgCt Background countrate ct/s/arcmin2 ExpTime Exposure time s HR1 Hardness ratio 1 number=2 The hardness ratios are defined by: hr1 = ( B - A ) / ( B + A ) , where A = countrate in PHA range 11 - 41 (~0.1-0.4 keV) B = countrate in PHA range 52 - 201 (~0.5-2.0 keV) hr2 = ( D - C ) / ( D + C ) , where C = countrate in PHA range 52 - 90 (~0.5-0.9 keV) D = countrate in PHA range 91 - 201 (~0.9-2.0 keV) (PHA = Pulse Height Amplitude) --- e_HR1 Error on HR1 --- HR2 hardness ratio 2 number=2 The hardness ratios are defined by: hr1 = ( B - A ) / ( B + A ) , where A = countrate in PHA range 11 - 41 (~0.1-0.4 keV) B = countrate in PHA range 52 - 201 (~0.5-2.0 keV) hr2 = ( D - C ) / ( D + C ) , where C = countrate in PHA range 52 - 90 (~0.5-0.9 keV) D = countrate in PHA range 91 - 201 (~0.9-2.0 keV) (PHA = Pulse Height Amplitude) --- e_HR2 Error on HR2 --- Extent Source extent, by which the source image exceeds the point spread function. --- L_Extent Likelihood of source extent --- ML Likelihood from maximum-likelihood method --- Ldetect Likelihood of source detection algorithm --- RibDist Distance to next rib or edge arcsec SrcDist Distance to next source before screening arcsec SrcDist2 Distance to next source after screening arcsec PrioFlags Source detection string number=3 the flags indicate the sliding window detection history using either the background map (M) or the local background (B), and take the values 0 = no detection, 1 = detection; The order of flags is: M-broad, L-broad, M-hard, L-hard, M-soft, L-soft --- PHA Source detection string number=4 the PHA (Pulse Height Amplitude) range PHA range with highest detection likelihood is indicated by A = PHA range 11-41 (~0.1-0.4 keV) B = PHA range 52-201 (~0.5-2.0 keV) C = PHA range 52-90 (~0.5-0.9 keV) D = PHA range 91-201 (~0.9-2.0 keV) b or blank means 'broad' --- Cell Detect cell size number=5 the basic detect cell size is 3x3 pixels, or 45x45arcsec; a value of 2 indicates a detect cell size of 90x90arcsec, a value of 4 indicates a detect cell size of 3x3arcmin, and a value of 8 a detect cell size of 6x6arcmin. 45arcsec VigFactor Vignetting factor number=6 the vignetting factor increases from 1 for sources detected on the axis to higher values when the source was detected off-axis. --- Confuse Confusion indicator --- Francois Ochsenbein CDS 1996 Jul 15 Thanks are due to Christian Motch <motch@astro.u-strasbg.fr> and Wolfgang Voges <whv@mpe-garching.mpg.de> for their help in the preparation of this document. UNKNOWN UNKNOWN From ftp://rosat_svc.mpe-garching.mpg.de/archive/sourcecat IX_11.xml The EINSTEIN Observatory Extended Medium-Sensitivity Survey (EMSS) 9015 IX/15 Einstein EMSS Survey The EINSTEIN Observatory Extended Medium-Sensitivity Survey (EMSS) I M Gioia T Maccacaro R E Schild A Wolter Astrophys. J. Suppl. Ser. 72 567 1990 1990ApJS...72..567G The EINSTEIN Observatory Extended Medium-Sensitivity Survey (EMSS) J T Stocke S L Morris I M Gioia T Maccacaro R E Schild A Wolter T A Fleming J P Henry Astrophys. J. Suppl. Ser. 76 813 1991 1991ApJS...76..813S IX/18 : EINSTEIN extended source survey (EXSS) (Oppenheimer+ 1997) Cleary, M.N., Heiles, C., and Haslam, C.G.T., 1979A&AS...36...95C Fleming, T.A. 1988, Ph. D. Thesis, University of Arizona Gioia, I.M., Maccacaro, T., Schild, R.E., Stocke, J.T., Liebert, J.W., Danziger, I.J., Kunth, D., & Lub, J., 1984ApJ...283..495G Gioia, I.M., Maccacaro, T., Morris, S.L., Schild, R.E., Stocke, J.T., Wolter, A., & Henry, P.H., 1990ApJS...72..567G Heiles, C. and Cleary, M.N., 1979, Australian J.Pys. Ap. Suppl, 47, 1. Maccacaro, T., & al. 1982ApJ...253..504M Maccacaro, T., Gioia, I.M., Wolter, A., Morris, S.L., & Stocke, J.T., 1988, 1988ApJ...326..680M Raymond, J.C. & Smith, B.W., 1977ApJS...35..419R Stark, A.A., Heiles, C., Bally, J., and Linker, R., 1989, Bells Lab, privately distributed magnetic tape Stocke, J.T., Liebert, J., Gioia, I.M., Griffiths, R.E., Maccacaro, T., Danziger, I.J., Kunth, D., & Lub, J., 1983ApJ...273..458S Stocke, J.T., Morris, S.L., Gioia, I.M., Maccacaro, T., Schild, R.E., Wolter, A., Fleming, T.A., & Henry, J.P., 1991ApJS...76..813S X-ray sources Active gal. nuclei BL Lac objects Clusters, galaxy Galactic plane The Einstein Extended Medium Sensitivity Survey (EMSS) consists of 835 serendipitous X-ray sources detected at or above 4 times the rms level in 1435 IPC fields with their centers located away from the galactic plane. Their limiting sensitivities range from ~5*10-14 to to ~ 3*10-12 erg.cm-2.s-1 in the 0.3-3.5keV band. A total area of 778 square degrees of the high galactic latitude sky (|b|>20) has been covered. The analysis has been performed using data from the Rev 1 processing system at the CfA. The resulting EMSS catalog is a flux-limited and homogeneous sample of astronomical objects that can be used for statistical studies. Here we present the table listing all the sources taken from the publication referenced below and the optical identifications. At present over 96% of the 835 X-ray sources have been successfully identified in the following proportions: active galactic nuclei (QSO's, quasars and Seyfert), 51.1%; BL Lacertae objects, 4.3%; clusters of galaxies, 12.2%; normal galaxies, 2.1%; cooling flow galaxies, 0.6%; Galactic stars 25.8%; and unidentified, 3.9%. Most of the individual optical counterparts are previously unknown objects and so constitute large statistical samples independent of previously selection methods. The contents of the table is described below. The sky coverage computed for a specific assumed source spectrum is also given under "Additional Information" below. For further details please see the published articles: Gioia et al. 1990, Stocke et al. 1991. Additional Information: The EMSS sky coverage. ---------------------- This sky coverage has been produced using the counts in the standard detection algorithm and assuming a power law spectrum with energy index = 1 and the measured Galactic hydrogen column density in the direction of each IPC pointing. We caution the user that this sky coverage is not appropriate for computation of functions like logN(>S)-logS, or Luminosity Functions of resolved sources, like clusters of galaxies or "normal" galaxies, nor of stars. The fluxes for these objects have been calculated either using extended counts, when appropriate, and/or different assumptions for the incident spectrum (see below). Limiting Sensitivity Area Covered (erg/cm**2/s) (sq. deg) 5.08E-14 0.09 6.09E-14 0.72 7.31E-14 2.54 8.78E-14 6.37 1.05E-13 15.1 1.26E-13 29.4 1.52E-13 55.2 1.82E-13 94.2 2.18E-13 139.4 2.62E-13 191.6 3.14E-13 249.5 3.77E-13 319.1 4.53E-13 402.0 5.43E-13 497.0 6.52E-13 582.9 7.83E-13 657.7 9.39E-13 711.8 1.13E-12 743.7 1.35E-12 762.7 1.62E-12 771.9 1.95E-12 775.7 2.34E-12 777.4 2.80E-12 777.9 3.36E-12 778.1 --------------------------------------------------------------------------------
Einstein
EMSS Catalogue name Name of EMSS source This column gives the source name; denoted by MS, followed by right ascension in hours, minutes, and truncated fraction of minutes, then declination in degrees and arcminutes (i.e. MS0013.4+1558). --- RAh Right Ascension (B1950.0) hours The right ascension and declination (B1950) correspond to the centroid of the X-ray source. h RAm RA minutes min RAs RA seconds s DE- Declination sign (B1950.0) --- DEd Dec degrees deg DEm Dec arcmin arcmin DEs Dec arcsec arcsec e_pos Positional Uncertainty The e_pos column gives the positional uncertainty, in arcseconds, the error associated with the position (90% confidence error circle radius). A positional uncertainty of 4" indicates sources detected also by the HRI. In these cases the coordinates of the source come from the HRI. arcsec x Position offset between optical and X-ray The offset in position between the X-ray centroid and the proposed optical counterpart in arcseconds of R.A. (x) and dec (y). Negative offsets indicate directions west and south of the X-ray centroids. Most of the offsets were measured automatically on the POSS or SRC J plates. They are accurate to +/- 5". For the SAO stars we have used the equinox 1950, epoch 1980 positions from the SAO catalog. When the optical counterpart is a radio source (Column <fR>), the VLA radio position is used (+/-1"). If more than one optical object is visible on the POSS within 10" of the offset position listed in this column, the identity of the optical counterpart is clarified with a note in the note column. When the optical counterpart is a cluster of galaxies, the optical offset refers to the brightest cluster member. arcsec y Position offset between optical and X-ray arcsec fX X-ray flux (*1.E-13 ergs/cm**2/s or *1.E-16 W/m**2) in the 0.3-3.5 keV band These columns give the X-ray flux (in units of 10E-13 erg/cm**2/s) and the one sigma error on the X-ray flux in the 0.3-3.5 keV band. The ext_flag column is flagged with an asterisk ('*') if extended counts from the column cts_ext were used to calculate the X-ray flux. The error on the X-ray flux is from photon counting statistics only, and is computed as the square root of the total observed counts in the detection cell. The flux has been computed in the 0.3-3.5 keV band for consistency with previous work (note that the Rev.1 processing computes it in the 0.2-3.5 keV band). The following assumptions have been adopted: (a) For the AGN, BL Lac objects and unidentified sources; we have multiplied the corrected count rate given in the ctrate column by a conversion factor appropriate for a power law spectrum with an energy index alpha = 1.0 and with the measured Galactic hydrogen column density in the direction of each IPC pointing. (b) For unresolved galaxies and clusters of galaxies; the flux has been computed using an identical procedure but with a different conversion factor appropriate for a Raymond-Smith thermal spectrum (Raymond and Smith, 1977) with temperature of about 6 keV. The above assumptions are justified by the results of the analysis of the X-ray energy distribution of the EMSS sources performed by Maccacaro et al. (1988). A number of sources are resolved even with the moderate angular resolution of the IPC. They are mainly clusters of galaxies but also 3 galaxies, 8 AGN, and 3 BL Lacs. For the extragalactic population, the X-ray flux listed has been corrected ("de-reddened") for Galactic absorption. For stars we have adopted a constant conversion factor of 1 IPC count/s = 2E-11 erg/cm**2/s corresponding to a Raymond-Smith thermal spectrum with temperatures in the range 8E05 - 3E06 K and no correction for the hydrogen column density. Note that RS CVn and K and M flare stars usually have a second temperature component in the range 1 - 2E07 K which results in nearly identical conversion factors to those derived from the Raymond-Smith models over these temperature ranges (see also Fleming, 1988, for a discussion of flux estimate of X-ray selected stars). In the case of clusters of galaxies the flux estimate should be evaluated in a region of constant physical size (e.g. 1 Mpc). Such a procedure cannot be applied to the serendipitous EMSS clusters, especially to the nearby ones, given their proximity to the ribs (or edges) of the detector or, in some cases, to the target of the observation. For all the resolved sources identified with clusters of galaxies or galaxies, and flagged as extended in the ext_flag column, we have used the extended counts measured according to the procedure described below the cts_ext column to compute the flux. 10-16W/m2 ext_flag Flagged '*' if source is extended --- e_fX 1 sigma error on X-ray flux 10-16W/m2 ctrate Corrected IPC count rate This column gives the corrected IPC count rate in units of cts/kilosecond. The count rate is derived from the net counts given in the cts column (which are then corrected for vignetting, mirror scattering, and point response function scattering) and the livetime given in the live column, which has already been corrected for instrumental dead time. ct/ks sn Signal to Noise Ratio This column gives the signal-to-noise ratio (s/n) computed as the source counts divided by the square root of the sum of the source counts and the background counts: Source Counts / (Source Counts + Background Counts)**(1/2)] --- cts Uncorrected net counts in 0.2-3.5 keV The uncorrected net counts in the 0.2-3.5 keV band are given in the cts column. No correction has been applied to the counts. The e_cts column gives the error on the net counts, computed as the square root of the total observed counts in the detection cell. The cts/e_cts ratio is the signal-to-noise given in the previous column. The total background counts are given in the bkgcts column. --- e_cts Error on net counts --- live Corrected exposure time This column gives the livetime, the exposure time of the IPC observation, corrected for instrumental dead time. It is given in seconds. The second line gives the background counts. s bkgcts Total background counts --- seqno IPC sequence number of the image used This column gives the sequence number of the observation, a unique numeric identifier for each observation which was allocated sequentially at the time of proposal submission. It is an internal index used to key on all references to an observation. If the ext_flag column is flagged with an asterisk ('*') then extended counts from the column cts_ext were used to calculate the X-ray flux. The cts_ext column gives the net extended counts. For IPC sources, this means that counts were computed manually to include all counts belonging to the source. For sources resolved by the IPC, the observed counts have been computed manually within a region centered on the source and with a size evaluated case by case so as to contain all the counts belonging to the source itself. Background counts for these sources have been computed within this same area from the background map produced by the REV.1 processing. In these cases only the vignetting and mirror scattering corrections have been applied. At the edge of the IPC detector the point spread function becomes significantly degraded so that some sources appear to be extended even though they might not be. Observations with a higher resolution instrument (e.g. the HRI or ROSAT) are needed to decide whether the extension is true or an artifact of the degradation of the IPC point spread function. This distortion of the point spread function cannot be modeled easily, so indications that sources are extended when they are near the IPC edge cannot be always trusted. Since these sources include ones which are identified as AGN and BL Lac objects as well as clusters, the indication of extension should be regarded as tentative. --- cts_ext Net extended counts --- nH Hydrogen column density (*E+25 m^-2 or *E+21 cm^-2) The hydrogen column density along the line of sight to the IPC field target determined using the HI survey of Stark et al. (1989). For regions of sky not surveyed by Stark et al. (south of declination -42 deg) the surveys of Heiles and Cleary (1979) and Cleary Heiles and Haslam (1979) have been used. 10+25m2 Vmag Visual magnitude The V band magnitude of the counterpart. Some entries are from photoelectric aperture photometry (for the stellar sources, see Fleming, 1988 and the Bright Star Catalog) or from CCD photometry with the Whipple Observatory 24 inch (for the extragalactic sources). These are typically accurate to 0.01 mag. Other entries are from the literature or are estimated magnitudes (+/- 0.5 mag) from the STScI digitized sky survey plates. A value of 0.0 indicates that the source is still unidentified, so there is no magnitude listed. mag n_fR '<' for upper limit in fR --- fR Radio flux at 5 GHZ The radio flux or 5 sigma upper limit in mJy at 5 GHz for the optical counterpart mostly comes from VLA observations. When a cluster of galaxies is the X-ray counterpart, radio emission from any cluster galaxy within the cluster is listed here. mJy fX/fv Logarithm of X-ray to visual flux ratio The logarithmic X-ray to optical flux ratio calculated from the observed X-ray and visible fluxes by log (fX/fv) = log fX + V/2.5 +5.37 (Maccacaro et al. 1988). These values are used to determine whether the optical counterpart is plausible. For this reason the X-ray flux used for this computation is not the value in the fX column but is rather the X-ray flux computed prior to assigning an optical identification class to each source. These "raw" X-ray fluxes use an assumed spectral index of -0.5 for all sources and a correction for galactic extinction equal to 3 X 10**20 cm-2 for all sources. The V band magnitudes quoted in the mv column were used for this calculation. For sources identified with clusters of galaxies the fX/fv is not given (fX/fv = 0.0) since the fX does not take into account the extended flux where present, and the V magnitude refers to the brightest cluster galaxy. --- class Proposed identification class of the X-ray source (see below) The class column gives the proposed identification or classification of the X-ray source. The following abbreviations are used: AGN = Active Galactic Nucleus (quasar or Seyfert galaxy) CL = Cluster of galaxies *CL* = Cooling flow galaxy BL = BL Lac object GAL = "normal" galaxy STAR = star UNID = source still unidentified --- r_class Reference for class The r_class column gives the reference for identification or classification. Identifications come from either our own spectroscopic work (EMSS in the 2nd line) or from other authors' work as indicated in the r_class column. References to other authors are given when the proposed identification has been published even if additional spectroscopic observations may have been obtained by us. References in column r_class of emss table: (MSS1) Stocke, J.T., Liebert, J., Gioia, I.M., Griffiths, R.E., Maccacaro, T., Danziger, I.J., Kunth, D., & Lub, J., 1983, ApJ, 273, 458 (1983ApJ...273..458S) (MSS2) Gioia, I.M., Maccacaro, T., Schild, R.E., Stocke, J.T., Liebert, J.W., Danziger, I.J., Kunth, D., & Lub, J., 1984, ApJ, 283, 495 (1984ApJ...283..495G) (1) White, S., Silk, J., & Henry, J.P., 1981ApJ...251L..65W (2) Margon, B., Downes, R., & Chanan, G., 1985ApJS...59...23M (3) Pravdo, S., & Marshall, F., 1984ApJ...281..570P (4) Huchra, J., Davis, M., Latham, D., & Tonry, J., 1983ApJS...52...89H (5) Hewitt, A., & Burbridge, G., 1987ApJS...63....1H (6) Kriss, G., & Canizares, C., 1982ApJ...261...51K (7) Wolstencraft, R., Hu, W., Arp, H., & Scarrott, S., 1983,, MNRAS, 1983MNRAS.205...67W (8) Chanan, G., Margon, B., & Downes, R., 1981ApJ...243L...5C (9) Mundt, R., Walter, F., Feigelson, E., Finkenzeller, V., Herbig, G., & Odell, A., 1983ApJ...269..229M (10) Henry, J.P., Soltan, A., Briel, U., & Gunn, J., 1982ApJ...262....1H (11) Margon, B., Boronson, T., Chanan, G., Thompson, I., & Schneider, D., 1986PASP...98.1129M (12) Caillault, J., Helfand, D., Nousek, J., & Takalo, L., 1986, 1986ApJ...304..318C (13) Morris, S., Schmidt, G., Liebert, J., Stocke, J., Gioia, I., & Maccacaro, T., 1987ApJ...314..641M (14) Biermann, P., Schmidt, G., Liebert, J., Stockman, H., Tapia, S., Strittmatter, P., West, S., & Lamb, D., 1985ApJ...293..303B (15) Reichert, G., Mason, K., Thorstensen, J., & Bowyer, S., 1982, 1982ApJ...260..437R (16) J. Huchra & M. Postman (private communication) (17) de Vaucouleurs, G., de Vaucouleurs, A., & Corwin, H., 1976, Second Reference Catalogue of Bright Galaxies (Austin: University of Texas Press) (Cat. <VII/112>) (18) I.J. Danziger (private communication) (19) Maccagni, D., Garilli, B., Gioia, I.M., Maccacaro, T. Vettolani, G., & Wolter, A., 1988ApJ...334L...1M (20) Katgert, P., Thuan, T., & Windhorst, R., 1983ApJ...271....1K (21) Mason, K., Spinrad, H., Bowyer, S., Reichert, G., & Stauffer, J., 1981AJ.....86..803M (22) Hoessel, J., Gunn, J., & Thuan, T., 1980ApJ...241..486H (23) F. Walter (private communication) (24) Morris, S.L., Liebert, J., Stocke, J.T, Gioia, I.M., Maccacaro, T., Schild, R.E., & Wolter, A., 1990, ApJ, 383, 686 (1990ApJ...365..686M) (25) Chanan, G., Margon, B., Helfand, D., Downes, R., & Chance, D., 1982ApJ...261L..31C (26) Kowalski, M., Ulmer, M., & Cruddace, R., 1983ApJ...268..540K (27) Nesci, R., Gioia, I., Maccacaro, T., Morris, S., Perola, G., Schild, R., & Wolter, A., 1989ApJ...344..104N (28) Maia, M., DeCosta, L., Willmer, C., Pellegrini, P., & Rite, C., 1987AJ.....93..546M (29) Marschall, L., Stefanik, R., Nations, R., & Karshner, G., 1989, BAAS, 21, 1083 (1989BAAS...21.1083M) (30) Fleming, T.A., Gioia, I.M., & Maccacaro, T., 1989AJ.....98..692F (31) Robb, R., 1989, IBUS, Nos. 3346 and 3370 (32) R. Robb, private communication; (33) Carter, B., Inglis, I., Ellis, R., Efstathiou, G., & Godwin, J., 1985MNRAS.212..471C (34) Kurtz, M., Huchra, J., Beers, T., Geller, M., Gioia, I.M., Maccacaro, T., Schild, R., & Stauffer, J., 1985AJ.....90.1665K (35) Silva, D., Liebert, J., Stocke, J.T. & Aaronson M., 1985, 1985PASP...97.1096S --- z Redshift If the counterpart is extragalactic the redshift is listed (+/- 0.003). --- n 'n' if a note on the source is in file notes --- comment Miscellaneous information on the source This column gives miscellaneous information on the source (i.e. radio catalogued source, SAO name, X-ray variable source, IRAS source, EXOSAT source, etc.). The EXOSAT CMA position is reported with the positional accuracy in parentheses. EMSS sources already published as part of the MSS samples are labelled as MSS1 (Maccacaro et al. 1982 and Stocke et al. 1983) and MSS2 (Gioia et al. 1984). --- I.Gioia, F. Ochsenbein CDS P. Kuin ADC 1995 Jul 31 Contact: Isabella Gioia, Institute for Astronomy; gioia@galileo.ifa.hawaii.edu UNKNOWN UNKNOWN * 19-Jan-1993: Original version received from Isabella Gioia, table adapted by F.Ochsenbein[CDS] * 19-Jan-1993. Documentation reformatted to v1.4 of standard by Paul Kuin [ADC] 31-Jul-1995. * 29-Aug-1997: catalogue number changed from VII/152 to IX/15 (high energy data) IX_15.xml A survey of the EINSTEIN IPC Database for extended X-ray sources. 9018 IX/18 EINSTEIN extended source survey A survey of the EINSTEIN IPC Database for extended X-ray sources. B R Oppenheimer D J Helfand E J Gaidos Astron. J. 113 2134-2146 1997 1997AJ....113.2134O I/146 : Positions and Proper Motions (PPM-North) I/193 : Positions and Proper Motions (PPM-South) I/208 : Positions and Proper Motions (PPM-90000 Supplement) VII/4 : Abell and Zwicky Clusters of Galaxies IX/13 : 2E Catalogue (Harris+ 1994) IX/15 : Einstein extended medium-sensitivity survey (EMSS) telnet://einline@einline.harvard.edu/ : the EINLINE data-base X-ray sources Clusters, galaxy This catalog contains sources from data collected by the IPC on board the EINSTEIN Observatory. This survey is designed to find extended sources and diffuse emission rather than point sources. In addition, the source detection algorithm is substantially improved over that used by EMSS. Sources were searched using circular apertures up to 6.1arcmin. The catalog contains 1326 extended source candidates at high galactic latitude (|b| > 20{deg}).
Einstein
The EXSS Catalogue Name EXSS source name --- RArad Right Ascension (B1950.0) rad DErad Declination (B1950.0) rad cts1 IPC photon counts per second for the aperture 1 detection (0.000 = no detection) ct/s cts2 IPC photon counts per second for the aperture 2 detection (0.000 = no detection) ct/s cts3 IPC photon counts per second for the aperture 3 detection (0.000 = no detection) ct/s cts4 IPC photon counts per second for the aperture 3 detection (0.000 = no detection) ct/s S/N1 Signal to noise ratio for aperture 1 --- S/N2 Signal to noise ratio for aperture 2 --- S/N3 Signal to noise ratio for aperture 3 --- S/N4 Signal to noise ratio for aperture 4 --- dRA1 Offset in right ascension of the aperture 1 detection from the assumed object position (columns 1 and 2), which is found through the technique described in the paper arcsec dDE1 Offset in declination for aperture 1 arcsec dRA2 Offset in right ascension for aperture 2 arcsec dDE2 Offset in declination for aperture 2 arcsec dRA3 Offset in right ascension for aperture 3 arcsec dDE3 Offset in declination for aperture 3 arcsec dRA4 Offset in right ascension for aperture 4 arcsec dDE4 Offset in declination for aperture 4 arcsec PPM =-99 Star number from the Positions and Proper Motions (PPM) Catalog (<I/146>, <I/193> and <I/208>) for the star which is identified with the EXSS source. --- Vmag =-99.00 V band magnitude of the PPM star mag dRA11 =-99.00 Right ascension difference between PPM and EXSS positions arcsec dDE11 =-99.00 Declination difference between the PPM and EXSS positions arcsec EMSS EMSS source <IX/15> identified with the EXSS source --- Typ11 Type of the EMSS source (from EMSS catalog) --- S/N11 =-99.0 Signal to noise ratio of the EMSS source with the EMSS detection algorithm --- dRA12 =-99.00 Right ascension difference between the EMSS and the EXSS positions arcsec dDE12 =-99.00 Declination difference between the EMSS and the EXSS positions arcsec ZwCl Zwicky cluster of galaxies identified with the EXSS source (see cat. <VII/4>) --- Size =-99.0 Approximate size of the Zwicky cluster (from the Zwicky catalog) arcsec dRA13 =-99.00 Right ascension difference between ZwCl and EXSS positions. arcsec dDE13 =-99.00 Declination difference between ZwCl and EXSS positions. arcsec Abell Abell cluster of galaxies identified with the EXSS source (see cat. <VII/4>) --- dRA14 =-99.00 Right ascension difference between Abell and EXSS positions arcsec dDE14 =-99.00 Declination difference between Abell and EXSS positions arcsec Typ14 The type of the corresponding source in the EINLINE database that is identified with the EXSS source number=1 to enter the EINLINE service, telnet to einline.harvard.edu login as 'einline', with no password --- dRA15 =-99.00 Right ascension difference between EINLINE and EXSS positions arcsec dDE15 =-99.00 Declination difference between EINLINE and EXSS positions arcsec d2 The quadratic sum of dRA15 and dDE15 arcsec2 Jean-Marie Hameury, Francois Ochsenbein CDS 1997 Aug 27 UNKNOWN UNKNOWN From http://astro.caltech.edu/~bro/exss/exss.html IX_18.xml Southern HII Regions: an extensive study of radio recombination line emission J/A+A/171/261 J/A+A/171/261 Radio Recombination Lines of Southern HII Regions Southern HII Regions: an extensive study of radio recombination line emission J L Caswell R F Haynes Astron. Astrophys. 171 261 1987 1987A&A...171..261C H II regions Radial velocities Radio lines Radio sources Galaxy: structure HII regions radio recombination lines We tabulate velocities and other parameters of hydrogen recombination lines near 5 GHz (H109alpha and H110alpha) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5 GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5 GHz continuum brightness temperature exceeding 1 K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5 GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.
Hydrogen recombination line data GLON Galactic longitude number=1 Coordinates are the position of peak 5 GHz continuum intensity from Haynes et al. (1979AuJPA..48....1H). deg GLAT Galactic latitude number=1 Coordinates are the position of peak 5 GHz continuum intensity from Haynes et al. (1979AuJPA..48....1H). deg m_V Recombination line velocity component --- RAh Right Ascension (1950) number=1 Coordinates are the position of peak 5 GHz continuum intensity from Haynes et al. (1979AuJPA..48....1H). h RAm Right Ascension (1950) min RAs Right Ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) number=1 Coordinates are the position of peak 5 GHz continuum intensity from Haynes et al. (1979AuJPA..48....1H). deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Tc Peak 5 GHz continuum brightness temperature K u_Tc Uncertainty flag on Tc --- Diam1 Angular size (first dimension) number=2 Angular sizes quoted for small diameter sources are widths to half maximum intensity of the equivalent deconvolved Gaussian source. For large irregular sources the quoted sizes are the average major and minor dimensions, and are very approximate. arcmin u_Diam1 Uncertainty flag on Diam1 --- Diam2 Angular size (second dimension) number=2 Angular sizes quoted for small diameter sources are widths to half maximum intensity of the equivalent deconvolved Gaussian source. For large irregular sources the quoted sizes are the average major and minor dimensions, and are very approximate. arcmin u_Diam2 Uncertainty flag on Diam2 --- S 5 GHz continuum flux density Jy u_S Uncertainty flag on S --- V1-H2CO LSR velocity of H2CO absorption line, first velocity component km/s V2-H2CO LSR velocity of H2CO absorption line, second velocity component km/s V3-H2CO LSR velocity of H2CO absorption line, third velocity component km/s V4-H2CO LSR velocity of H2CO absorption line, fourth velocity component km/s nH2CO Note on H2CO measurements: ND: no detectable H2CO absorption, NA: no available H2CO measurement --- rH2CO Reference for H2CO results: CH: this survey, Caswell and Haynes (1987), WG: Whiteoak and Gardner (1974) and Gardner and Whiteoak (1984) --- TL Peak recombination line brightness temperature number=3 Determined from a Gaussian fit to the observed line profile. K u_TL Uncertainty flag on TL --- DV Width of recombination line, full width at half intensity number=3 Determined from a Gaussian fit to the observed line profile. km/s u_DV Uncertainty flag on DV --- V LSR velocity of recombination line number=3 Determined from a Gaussian fit to the observed line profile. km/s u_V Uncertainty flag on V --- Te LTE Electron Temperature K u_Te Uncertainty flag on Te --- Rg Galactocentric radius number=4 Derived from the recombination line LSR velocity assuming the Schmidt (1965) rotation curve inside the solar circle, a flat rotation curve (V= 250 km/s) outside the solar circle, and 10 kpc for the distance of the Sun from the Galactic center. Sources in the first or fourth quadrants with velocities exceeding, or within 5 km/s of, the terminal velocity as defined by the Schmidt rotation curve are assigned to the tangent point. kpc u_Rg Uncertainty flag on Rg --- d1 Kinematic distance, or near kinematic distance (4) number=5 For sources with two possible kinematic distance solutions, d1 contains the near distance and d2 contains the far distance. For other sources, d1 contains the kinematic distance and d2 is blank. kpc u_d1 Uncertainty flag on d1 --- d2 Far kinematic distance (4) number=5 For sources with two possible kinematic distance solutions, d1 contains the near distance and d2 contains the far distance. For other sources, d1 contains the kinematic distance and d2 is blank. kpc f_d1 Near/far preference flag, N: near kinematic distance is significantly more likely, F: far kinematic distance is significantly more likely --- n_d1 HI absorption flag, HI: near/far preference is based on 21 cm absorption line data --- ref Reference for recombination line results if cited from another source number=6 C: Caswell (1972), CC: Caswell and Clark (1975AuJPA.......57C), Ch: Churchwell et al. (1974A&A....32..283C), CHC: Caswell et al. (1975AuJPh..28..633C), HD: Huchtmeier and Day (1975A&A....41..153H), S: Shaver at el. (1983MNRAS.204...53S), W: Wilson et al. (1970A&A.....6..364W). --- Note Source comments, N indicates that section 4 of Caswell and Haynes (1987) contains additional information or discussion for this source --- Opt Optical counterpart number=7 'V', or a specific nebula name, denotes the presence of a visible optical counterpart, and 'A' indicates the absence of an optical counterpart. --- Nils Odegard SSDOO/ADC 1999 Aug 01 H. Andernach <Heinz.Andernach@astro.ugto.mx> and S. Trushkin scanned the published data table, made format changes, and provided a copy of their electronic version to ADC. J_A+A_171_261.xml The Cygnus X region. XVIII. A detailed investigation of radio continuum structure on large and small scales J/A+A/241/551 J/A+A/241/551 The Cygnus X region. XVIII. A detailed The Cygnus X region. XVIII. A detailed investigation of radio continuum structure on large and small scales H J Wendker L A Higgs T L Landecker Astron. Astrophys. 241 551 1991 1991A&A...241..551W Cygnus X HII regions radio sources supernova remnants surveys *** No Description Available ***
Small-diameter radio sources at 408 MHz Small-diameter radio sources at 1420 MHz Small-diameter radio sources at 4800 MHz Name Designation (The sources are designated as 18Pl(408 MHz), 19Pm(1420MHz) and ECX6-n(4800 MHz), where l, m and n are serial numbers in each list) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s e_RA rms uncertainty on right ascension s DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec e_DE rms uncertainty on declination arcsec Fi Integrated flux density mJy e_Fi rms uncertainty on flux density. If no value is given, the published table mentions (centroid) mJy Fp Peak flux. If no value is given, the published table mentions (integrated) mJy e_Fp rms uncertainty on peak flux mJy Maj Size along major axis arcmin Size Size along minor axis arcmin PA Position angle deg Derived source properties 18P 18P denomination of the source --- 19P 19P denomination of the source --- ECX6 ECX6 denomination of the source --- Beta Spectral index 408/4800 MHz --- Th Thermal (Th) or non-thermal (NT) source --- Ext Extended (E) source --- Res Resolution effects (R) --- Rem Remarks --- James Marcout, Patricia Bauer CDS 1994 Apr 22 UNKNOWN UNKNOWN keypunched at CDS J_A+A_241_551.xml Walraven photometry of WX Hyi during quiescence and outburst. J/A+A/242/401 J/A+A/242/401 Walraven photometry of WX Hyi during quiescence Walraven photometry of WX Hyi during quiescence and outburst. E Kuulkers A Hollander T Oosterbroek J Van Paradijs Astron. Astrophys. 242 401 1991 1991A&A...242..401K Accretion Novae Stars, double and multiple accretion, accretion disks binaries: close novae, cataclysmic variables *** No Description Available ***
VBLUW fluxes of WX Hyi BJED BJED - 2447000.00 number=1 Barycentric corrected Julian Ephemeris Date d V Flux in V-band number=2 Bad integrations have a value of -99. mJy B Flux in B-band number=2 Bad integrations have a value of -99. mJy L Flux in L-band number=2 Bad integrations have a value of -99. mJy U Flux in U-band number=2 Bad integrations have a value of -99. mJy W Flux in V-band number=2 Bad integrations have a value of -99. mJy Francois Ochsenbein CDS 1993 Feb 11 J_A+A_242_401.xml The spectrum of the VV Cep star KQ Puppis (Boss 1985). IV. The Fe II spectrum, level population and spectral synthesis J/A+A/258/423 J/A+A/258/423 Fe II spectrum, level population and spectral The spectrum of the VV Cep star KQ Puppis (Boss 1985). IV. The Fe II spectrum, level population and spectral synthesis G Muratorio R Viotti M Friedjung G B Baratta C Rossi Astron. Astrophys. 258 423 1992 1992A&A...258..423M atomic processes binaries: general binaries: spectroscopic line: formation molecular processes stars: emission-line, Be Results of an analysis of the intensities of the numerous Fe II emission and absorption lines present in the UV spectrum of KQ Puppis are reported. The self-absorption curve method developed by Friedjung and Muratorio (1987) is used to analyze the emission line intensities. The Fe II terms with chi from 0 to 11.5 eV are found to be populated according to a Boltzmann-type law with a mean excitation temperature of 9000 +/- 700 K. Above about 8 eV many terms show a population excess which can be attributed to a significant contribution of dielectronic recombination, and to fluorescence effects. The lower limit to the cool component mass loss rate is estimated at (4 +/- 2) x 10 exp -6 solar mass/yr.
The spectrum A/E Nature of the line: A = absorption, E = emission. --- Lab Laboratory wavelength (in A) of the transition. 0.1nm Log.gf Log gf (from Kurucz 1981). --- E.P. Excitation potential of the lower level. cm-1 JL J number of the lower level. --- JU J number of the upper level. --- MULT Multiplet number according to Moore (1945) and Moore (1950), labeled with "o". "K" denotes a transition listed by Kurucz (1981). --- F1 Emission line flux in 10-13 erg cm-2 s-1 corrected for an interstellar extinction of E(B-V)=0.14 measured in the February 1979 IUE spectrum. 10-16W/m2 u_F1 Uncertainty flag (:) on F1, or S for saturated p for a transition contributing to the previous flux --- W1 Equivalent width (in mA) in February 1979. 0.1pm u_W1 Uncertainty flag on W1 (as in col. 49) --- F2 Dereddened emission line flux in February 1980. 10-16W/m2 u_F2 Uncertainty flag on F2 (as in col. 49) --- W2 Equivalent width in February 1980. 0.1pm u_W2 Uncertainty flag on W2 (as in col. 49) --- Rem Remarks: bl = more than one transition contribute to the line. (indicated with "...") broad = broad spectral feature. opt = optical transition (Moore 1945). R.M. = IUE reseau mark. --- Francois Ochsenbein CDS 1993 Feb 19 J_A+A_258_423.xml The radial structure of the galactic disc J/A+A/265/32 J/A+A/265/32 The radial structure of the galactic disc The radial structure of the galactic disc A C Robin M Creze V Mohan Astron. Astrophys. 265 32 1992 1992A&A...265...32R Galactic plane Photometry Populations, stellar anticenter Galaxy: structure photometry stellar populations, galactic disk Deep CCD photometry has been performed in four CCD frames inside Kapteyn's special Selected Area 53, which is known as a low extinction Window of the Galactic Anticenter. The catalogues of stellar objects detected in 4 CCD fields brighter than V = 25 are given in field1 to field4 Columns 2 and 3 give the position in equatorial coordinates for equinox 2000.0 Columns 4 to 6 give the magnitude and colours transformed to the Johnson system.
Positions and UBV, field 1 (V <= 25) Positions and UBV, field 2 (V <= 25) Positions and UBV, field 3 (V <= 25) Positions and UBV, field 4 (V <= 25) NUMBER Running number --- RAh J2000 right ascension h RAm J2000 right ascension min RAs J2000 right ascension s DE- J2000 declination --- DEd J2000 declination deg DEm J2000 declination arcmin DEs J2000 declination arcsec V V magnitude transformed to Johnson system mag B-V B-V color index (Johnson system) mag U-B U-B color index (Johnson system) mag CDS 1993 Mar 02 J_A+A_265_32.xml Quasi-periodic oscillations in TT Ari J/A+A/265/77 J/A+A/265/77 VBLUW Observations of TT Ari Quasi-periodic oscillations in TT Ari A Hollander J Van Paradijs Astron. Astrophys. 265 77 1992 1992A&A...265...77H J/A+A/265/77 : (TT Ari) J/A+AS/101/87 : (BV Cen, HL Aqr, V26 Oph, V603 Aql, V2051 Oph, V3885 Sgr, VY Scl, WW Cet) accretion, accretion disks novae, cataclysmic variables photometry stars: individual (TT Ari) X-rays: binaries *** No Description Available ***
VBLUW fluxes of TT Ari BJED Barycentric corrected Julian Ephemeris Date d V =-99. Flux in V-band number=1 Bad integrations have a value of -99. mJy B =-99. Flux in B-band number=1 Bad integrations have a value of -99. mJy L =-99. Flux in L-band number=1 Bad integrations have a value of -99. mJy U =-99. Flux in U-band number=1 Bad integrations have a value of -99. mJy W =-99. Flux in V-band number=1 Bad integrations have a value of -99. mJy Francois Ochsenbein CDS 1995 Jul 05 UNKNOWN UNKNOWN * 11-Feb-1993: first archived * 05-Jul-1995: converted the documentation; replaced the original BJED which was starting at 2447000.00 by the full date J_A+A_265_77.xml The atmospheric parameters of A and F stars. I. Comparison of various methods J/A+A/271/515 J/A+A/271/515 The atmospheric parameters of A and F stars. I The atmospheric parameters of A and F stars. I. Comparison of various methods B Smalley M M Dworetsky Astron. Astrophys. 271 515 1993 1993A&A...271..515S Photometry, H-beta Photometry, H-gamma Stars, A-type Stars, atmospheres Stars, F-type line: profiles stars: chemically peculiar stars: fundamental parameters techniques: photometric *** No Description Available ***
H beta profiles H gamma profiles HR number --- HD number --- R1 Residual flux at 1 angstrom from line core --- R2 Residual flux at 2 angstroms from line core --- R4 Residual flux at 4 angstroms from line core --- R6 Residual flux at 6 angstroms from line core --- R8 Residual flux at 8 angstroms from line core --- R10 Residual flux at 10 angstroms from line core --- R15 Residual flux at 15 angstroms from line core --- R20 Residual flux at 20 angstroms from line core --- R25 Residual flux at 25 angstroms from line core --- R30 Residual flux at 30 angstroms from line core --- R35 Residual flux at 35 angstroms from line core --- R40 Residual flux at 40 angstroms from line core --- CDS 1993 Feb 09 J_A+A_271_515.xml Star formation in L1251: distance and members J/A+A/272/235 J/A+A/272/235 Star formation in L1251: distance and members Star formation in L1251: distance and members T Kun M Prusti Astron. Astrophys. 272 235 1993 1993A&A...272..235K infrared: stars ISM: individual (L 1251) stars: formation stars: pre-main sequence *** No Description Available ***
Field stars around L1251 Number Serial number --- Sp Spectral type --- V V magnitude mag B-V B-V colour index mag E(B-V) colour excess mag y Distance modulus mag H alpha emission stars L1251 Number Serial number --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec V V magnitude mag V-R Color mag R-I Color mag I(Ha) s:strong w:weak --- IRAS point sources in L1251 Number Sequence number --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec l_F(12) < for upper limit --- F(12) IRAS flux at 12 mum Jy l_F(25) < for upper limit --- F(25) IRAS flux at 25 mum Jy l_F(60) < for upper limit --- F(60) IRAS flux at 60 mum Jy l_F(100) < for upper limit --- F(100) IRAS flux at 100 mum Jy Name Name --- CDS 1993 Mar 27 J_A+A_272_235.xml The ultraviolet to soft X-ray bump of Seyfert 1 type Active Galactic Nuclei J/A+A/274/105 J/A+A/274/105 The ultraviolet to soft X-ray bump of Seyfert 1 typ The ultraviolet to soft X-ray bump of Seyfert 1 type Active Galactic Nuclei R Walter H H Fink Astron. Astrophys. 274 105 1993 1993A&A...274..105W Galaxies, Seyfert Ultraviolet X-ray sources galaxies: Seyfert ultraviolet: galaxies X-rays: galaxies *** No Description Available ***
All parameters N Sequence number --- Name Source name --- RAh Position 1950 h RAm Position 1950 min DE- Position 1950 - DEd Position 1950 deg DEm Position 1950 arcmin z Redshift --- gNH Galactic column density 10+21/cm2 F2675 Dered. 2675A flux density (source rest frame) (E-11erg/s/cm2) 10-14W/m2 pna2675 Fix Pattern noise amplitude at 2675A 10-14W/m2 F1375 Dered. 1375A flux density (source rest frame) (E-11erg/s/cm2) 10-14W/m2 pna1375 Fix Pattern noise amplitude at 1375A 10-14W/m2 F5GHz 5GHz flux density (E-14erg/s/cm2) 10-17W/m2 F25mum 25micron flux density (E-11erg/s/cm2) 10-14W/m2 gam-ind Index 2-10keV photon index --- e_gam-ind+ Positive uncert. or var. of 2-10keV photon index --- e_gam-ind- Negative uncert. or var. of 2-10keV photon index --- PSPC Upper PSPC channel --- sX_ind Soft X-ray photon index (free NH fit) --- e_sX_ind Soft X-ray photon index uncertainty (free NH) --- aNH Absorbing column density for pwl model 10+21H/cm2 e_aNH Absorbing column density uncertainty 10+21H/cm2 F2-NH 2keV flux density (free NH fit) (E-11erg/s/cm2) 10-14W/m2 e_F2-NH 2keV flux density uncertainty 10-14W/m2 chi2_F2-NH Reduced chi-square for free NH fit --- NHl-bb NH fitted at low energy with black body model 10+21H/cm2 e_NHl-bb Error on NH fitted at low energy with black body model 10+21H/cm2 NHl-bs NH fitted at low energy with thermal Bremsstrahlung model 10+21H/cm2 e_NHl-bs Error on NH fitted at low energy with thbr 10+21H/cm2 F2-2com 2keV flux density for two components model (E-11erg/s/cm2) 10-14W/m2 e_F2-2c 2keV flux density error for 2Comp. model 10-14W/m2 E(sX) Soft X-ray excess for two components model --- e_EsX+ Positive uncertainty on Soft X-ray excess --- e_EsX- Negative uncertainty on Soft X-ray excess --- chi2_2c Reduced chi-square for two components model --- sXind Soft X-ray photon index (fixed NH fit) --- e_sXind Soft X-ray photon index uncertainty (fixed NH) --- chi2_sXind Reduced chi-square for fixed NH fit --- CDS 1993 Apr 05 J_A+A_274_105.xml Elemental abundances in normal late-B and HgMn stars from co-added IUE spectra. I. Iron-peak elements J/A+A/274/335 J/A+A/274/335 Elemental abundances in normal late-B and HgMn stars Elemental abundances in normal late-B and HgMn stars from co-added IUE spectra. I. Iron-peak elements K C Smith M M Dworetsky Astron. Astrophys. 274 335 1993 1993A&A...274..335S Stars, Ap Stars, B-type Stars, normal Ultraviolet stars: abundances stars: atmospheres stars: chemically peculiar stars: early-type ultraviolet: stars *** No Description Available ***
Basic data and adopted atmospheric parameters Type N: normal star, H: HgMn star, S: superficially normal star --- Star Star name --- HD HD number --- Sp Spectral type --- Vr Velocity km/s n_Vr see note number=1 Spectral types and radial velocity data from Hoffleit & Jaschek (1982, The Bright Star Catalogue. Yale Univ. Observatory, Connecticut, USA) with revisions according to Hoffleit (1984, Bull. Inform. CDS No. 26, p.161) and Stickland & Weatherby (1984, A&AS, 57, 55). 'V' and 'V?': known and suspected radial velocity variables respectively; 'SB': spectroscopic binary ('SB1' and 'SB2' denote single- and double-lined systems respectively); 'O': published orbit (see Batten et al. 1989, Publs. Dom. astrophys. Obs. 17, 1). --- NIUE Number of co-added high-resolution long-wavelength IUE spectra --- Teff Effective temperature K log(g) Surface gravity cm/s2 xi Microturbulence parameter km/s u_xi If ':' microturbulence parameter derived from UV Fe II lines --- r_xi Reference for microturbulence parameter number=2 References: [1] Adelman & Fuhr (1985, A&A, 152, 434) [2] Adelman (1988, MNRAS, 235, 749) [3] Smith (1992, Ph.D. Thesis, University of London) [4] Gigas (1986, A&A, 165, 170) [6] Adelman (1989, MNRAS, 239, 487) [7] Dworetsky & Coates (personnal communication) [8] Adelman (1988, MNRAS, 235, 763) [9] Cowley (1980, PASP, 92, 159) [10] White et al. (1976, ApJ, 204, 131) [11] Adelman (1987, MNRAS, 228, 573) [12] Dworetsky (1971, Ph.D. Thesis, University of California, Los Angeles) [13] Castelli et al. (1985, A&AS, 59, 1) --- Vsini Rotational velocity km/s r_Vsini Reference for rotational velocity number=2 References: [1] Adelman & Fuhr (1985, A&A, 152, 434) [2] Adelman (1988, MNRAS, 235, 749) [3] Smith (1992, Ph.D. Thesis, University of London) [4] Gigas (1986, A&A, 165, 170) [6] Adelman (1989, MNRAS, 239, 487) [7] Dworetsky & Coates (personnal communication) [8] Adelman (1988, MNRAS, 235, 763) [9] Cowley (1980, PASP, 92, 159) [10] White et al. (1976, ApJ, 204, 131) [11] Adelman (1987, MNRAS, 228, 573) [12] Dworetsky (1971, Ph.D. Thesis, University of California, Los Angeles) [13] Castelli et al. (1985, A&AS, 59, 1) --- Mean abundances for iron-peak elements Type N: normal star, H: HgMn star S: superficially normal star --- Star Star name --- HD HD number --- A(Cr) Cr abundance number=1 Abundances are given on a scale where log N(H)= 12. Quoted uncertainties are formal standard errors --- e_A(Cr) rms uncertainty on Cr abundance --- A(Mn) Mn abundance number=1 Abundances are given on a scale where log N(H)= 12. Quoted uncertainties are formal standard errors --- e_A(Mn) rms uncertainty on Mn abundance --- A(Fe) Fe abundance number=1 Abundances are given on a scale where log N(H)= 12. Quoted uncertainties are formal standard errors --- e_A(Fe) rms uncertainty on Fe abundance --- l_A(Co) limit flag on Co abundance --- A(Co) Co abundance number=1 Abundances are given on a scale where log N(H)= 12. Quoted uncertainties are formal standard errors --- e_A(Co) rms uncertainty on Co abundance --- A(Ni) Ni abundance number=1 Abundances are given on a scale where log N(H)= 12. Quoted uncertainties are formal standard errors --- e_A(Ni) rms uncertainty on Ni abundance --- Patricia Bauer CDS 1993 Sep 20 J_A+A_274_335.xml A study of the asymmetry of Fe I lines in the solar spectrum J/A+A/274/555 J/A+A/274/555 A study of the asymmetry of Fe I lines in the A study of the asymmetry of Fe I lines in the solar spectrum M Stathopoulou C E Alissandrakis Astron. Astrophys. 274 555 1993 1993A&A...274..555S Line Profiles Sun line: profiles Sun: granulation Sun: photosphere *** No Description Available ***
Measures of 75 Fe I lines --- Serial number of line --- Lambda Wavelength of line 0.1nm Chi Excitation potential eV I0(1.0) Central line intensity % I0(0.2) Central line intensity % I0(flux) Central line intensity % W(1.0) Equivalent width 0.1pm W(0.2) Equivalent width 0.1pm W(flux) Equivalent width 0.1pm logTau_0(1.0) Log of optical depth at line center --- logTau_0(0.2) Log of optical depth at line center --- logTau_m(flux) Log of optical depth at line center --- logTau_m(1.0) Log of mean optical depth --- logTau_m(0.2) Log of mean optical depth --- logTau_m(flux) Log of mean optical depth --- <Alpha>(1.0) Median value of line asymmetry m/s <Alpha>(0.2) Median value of line asymmetry m/s <Alpha>(flux) Median value of line asymmetry m/s Alpha_m(1.0) Mean line asymmetry m/s Alpha_m(0.2) Mean line asymmetry m/s Alpha_m(flux) Mean line asymmetry m/s Patricia Bauer CDS 1993 Sep 16 J_A+A_274_555.xml Radio continuum observations of southern planetary nebulae candidates J/A+A/274/895 J/A+A/274/895 Radio continuum obs of southern planetary Radio continuum observations of southern planetary nebulae candidates G C M Van De Steene S R Pottasch Astron. Astrophys. 274 895 1993 1993A&A...274..895V Interstellar medium Nebulae, planetary Radio sources infrared: ISM: continuum planetary nebulae: general radio continuum: ISM *** No Description Available ***
Far infra-red data of the observed sources IRAS IRAS designation number=1 the original name was replaced at CDS by the true IRAS name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec F12 IRAS flux at 12 um Jy F25 IRAS flux at 25 um Jy F60 IRAS flux at 60 um Jy F100 IRAS flux at 100 um Jy FQual Qualities from IRAS (3=good) --- Tc Color temperature number=1 the original name was replaced at CDS by the true IRAS name K FIR Total far infra-red flux number=1 the original name was replaced at CDS by the true IRAS name 10-23W/m2 e_FIR rms error on FIR W/m2 detected 'y' indicates a detection in radio continuum (table3) --- Radio data of the detected sources IRAS IRAS designation number=1 the original name was replaced at CDS by the true IRAS name --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right Ascension 1950 (hours) of radio source h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) of radio source - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Dist Distance between IRAS and radio sources arcsec S6cm Radio continuum 6cm flux density mJy e_S6cm error estimate on S6cm mJy l_FWHM Limit flag on FWHM --- FWHM radio gaussian diameter at FWHM arcsec l_Diam Limit flag on Diam --- Diam Actual diameter arcsec l_Tb Limit flag on Tb --- Tb Brightness temperature K IRE InfraRed Excess, ratio of total far-IR flux to the radio flux --- James Marcout, Francois Ochsenbein CDS 1994 Feb 04 UNKNOWN UNKNOWN keypunched at CDS J_A+A_274_895.xml The chemical evolution of the galactic disk I. Analysis and results J/A+A/275/101 J/A+A/275/101 The chemical evolution of the galactic disk I. The chemical evolution of the galactic disk I. Analysis and results B Edvardsson J Andersen B Gustafsson D L Lambert P E Nissen J Tomkin Astron. Astrophys. 275 101 1993 1993A&A...275..101E Galaxy: evolution Galaxy: kinematics and dynamics Galaxy: structure stars: atmospheres stars: fundamental parameters *** No Description Available ***
Atomic line data and solar equivalent widths Element Line identification: chemical element and ionization stage --- Lambda Wavelength (Angstroms) 0.1nm E Line excitation energy eV log.gf Log gf (oscillator strength) --- Factor Enhancement factor to the "classical van der Waals damping Gamma_6" --- Damping Radiation damping constant Hz W Solar flux spectrum equivalent width (milliAngstrom). The measured equivalent widths were corrected for 1% scattered light by multiplication by the factor 1.01 as described in Sect.2 of PaperII. 0.1pm Source for Solar equivalent width: E=ESO spectrum, M=McDonald spectrum --- Fundamental data and chemical abundances of 14 species for the programme stars Name Star catalogue, HR or HD --- Teff Effective temperature K log.g Logarithmic surface gravity cm/s2 [Me/H] overall photometric metallicity derived for the stars, normalized on the Sun ([Me/H] values closer to the resulting [Fe/H] values were used for the models of 15 stars, cf. Sect.3.1.1. [Me/H] values for these 15 are given with a colon corresponding to parantheses in the printed version) --- u_[Me/H] Uncertainty flag (:) on Me/H (Note: values are within parantheses in the printed version) --- [Fe/H] resulting spectroscopic iron abundance (derived from lines of Fe I), normalized to the Sun --- R Heliocentric distance pc U Heliocentric velocity (U is positive towards the galactic anti-centre), km/s V Heliocentric velocity (V is positive in the direction of circular motion) km/s W Heliocentric velocity (W is positive towards the galactic north pole) km/s Rp Perigalactic distance kpc Rm Straight mean of the perigalactic and the apogalactic distances kpc Zmax Maximum distance from the galactic plane kpc e Orbital eccentricity as projected on the galactic plane --- log.age Logarithm of the stellar age (in Gigayears) determined from isochrones NOTE that this parameter is missing for 7 stars Ga Rem Remarks: SB = spectroscopic binaries (with possibly uncertain distances), pm = stars with uncertainties in proper motions significantly above 0.005 arcsecs per year h = possible hook stars (for which the ages may be underestimated by 0.15 dex). --- [FeI/H] Chemical abundance (normalized to the Sun) --- [OI/H] Chemical abundance (normalized to the Sun) --- [NaI/H] Chemical abundance (normalized to the Sun) --- [MgI/H] Chemical abundance (normalized to the Sun) --- [AlI/H] Chemical abundance (normalized to the Sun) --- [SiI/H] Chemical abundance (normalized to the Sun) --- [CaI/H] Chemical abundance (normalized to the Sun) --- [TiI/H] Chemical abundance (normalized to the Sun) --- [FeII/H] Chemical abundance (normalized to the Sun) --- [NiI/H] Chemical abundance (normalized to the Sun) --- [YII/H] Chemical abundance (normalized to the Sun) --- [ZrII/H] Chemical abundance (normalized to the Sun) --- [BaII/H] Chemical abundance (normalized to the Sun) --- [NdII/H] Chemical abundance (normalized to the Sun) --- [alpha/H] = 0.25([Mg/H] + [Si/H] + [Ca/H] + [Ti/H]) --- CDS 1993 May 18 J_A+A_275_101.xml Probing the AGB tip: luminous carbon stars in the galactic plane J/A+A/275/163 J/A+A/275/163 Probing the AGB tip: luminous carbon stars in the Probing the AGB tip: luminous carbon stars in the galactic plane J H Kastner T Forveille B Zuckerman A Omont Astron. Astrophys. 275 163 1993 1993A&A...275..163K circumstellar matter radio lines: stars stars: AGB and post-AGB stars: carbon stars: evolution surveys *** No Description Available ***
Sources observed in CO Name IRAS name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLON Galactic longitude (lII) deg GLAT Galactic latitude (bII) deg Flux IRAS fluxes: F12,F25,F60 Jy Type IRAS LRS type. Letter designations refer to classification in Volk et al., 1991, ApJS 77, 607 I= noisy/incomplete, F= featureless C= SiC emission, E= silicate emission U= unusual --- Index IRAS variability index --- Name Other object designations --- CO observations: results Name IRAS name --- TB.V(1-0) CO(1-0) line area K.km/s l_TB.V(1-0) CO(1-0) upper limit flag --- TB(1-0) CO(1-0) peak antenna temperature TB K V(LSR)(1-0) CO(1-0) LSR velocity km/s Vexp(1-0) CO(1-0) expansion velocity km/s TB.V(2-1) CO(2-1) line area K.km/s l_TB.V(2-1) CO(2-1) upper limit flag --- TB(2-1) CO(2-1) peak antenna temperature TB K V(LSR)(2-1) CO(2-1) LSR velocity km/s Vexp(2-1) CO(2-1) expansion velocity km/s Near-IR photometry of CO sources Name IRAS name --- J J(1.25 micron) flux, uncorrected mJy H H(1.65 micron) flux, uncorrected mJy K K(2.2 micron) flux, uncorrected mJy L L(3.5 micron) flux, uncorrected mJy Jc J(1.25 micron) flux, corrected mJy Hc H(1.65 micron) flux, corrected mJy Kc K(2.2 micron) flux, corrected mJy Lc L(3.5 micron) flux, corrected mJy r_flux Reference flag (see note) --- Detections of SiO, H2O and HCN Name IRAS name --- Molecule Molecule name --- TB Peak antenna temperature TB K V_0 LSR velocity km/s DeltaV Line width; for SiO and H2O detection, full width at half maximum, for HCN, half width at zero power km/s Kinematic distances, bolometric fluxes, luminosities Name IRAS name --- Type Type --- Dkin Near kinematic distance kpc Fbol Bolometric flux, uncorrected mW/m2 L Luminosity, uncorrected Sun Fbol,0 Bolometric flux, corrected mW/m2 L_0 Luminosity, corrected Sun Fbol,BC Bolometric flux from (12-25) color mW/m2 L_BC Luminosity from (12-25) color Sun Patricia Bauer CDS 1993 Sep 21 J_A+A_275_163.xml Stroemgren photometry of dwarf novae J/A+A/275/201 J/A+A/275/201 Stroemgren photometry of dwarf novae Stroemgren photometry of dwarf novae J Echevarria R Costero R Miche Astron. Astrophys. 275 201 1993 1993A&A...275..201E dwarf novae novae, cataclysmic variables Photometry *** No Description Available ***
The dwarf novae Object Variable name --- y y magnitude mag b-y b-y color mag m_1 m_1 color mag c_1 c_1 color mag beta beta color mag Date Observation date --- Type Dwarf novae type --- State The entries refer to: minimum (m), rise (R), maximum (M), decline (D) and standstill (S) --- The comparison stars Object "C" followed by variable name which was studied --- x x position in referenced charts mm y y position in referenced charts mm Ref Reference to charts : (1) Vogt & Bateson, 1982, A&AS, 48, 383 (2) Bruch et al., 1987, A&AS, 190, 119 --- Note (a) TZ Per is wrongly identified in the chart. The correct position is at 3.5, 0.5 from the center of the chart --- y y magnitude mag b-y b-y color mag m_1 m_1 color mag c_1 c_1 color mag beta beta color mag Sp Spectral type derived from photometry --- Patricia Bauer CDS 1993 Sep 16 J_A+A_275_201.xml The double-mode semiregular variable UU Herculis: 1990-1992 photometry J/A+A/275/484 J/A+A/275/484 The double-mode semiregular variable UU Herculis: The double-mode semiregular variable UU Herculis: 1990-1992 photometry E Zsoldos J D Fernie A Arellano-Ferro S Seager Astron. Astrophys. 275 484 1993 1993A&A...275..484Z stars: individual (UU Her) stars: oscillations stars: variables: general *** No Description Available ***
V and (b-y) photometry of UU Her JD Julian day-2440000 d V magnitude mag (b-y) colour mag UBV photometry of UU Her Julian date-2440000 d V magnitude mag u_V Uncertainty flag (:) on V --- (B-V) colour mag u_(B-V) Uncertainty flag (:) on (B-V) --- (U-B) colour mag u_(U-B) Uncertainty flag (:) on (U-B) --- BVRI photometry of UU Her Julian date-2440000 d V magnitude mag (B-V) colour mag (V-R) colour mag (V-I) colour mag uvbybeta photometry of UU Her Julian date-2440000 d V magnitude mag u_V Uncertainty flag (:) on V --- (b-y) colour mag u_(b-y) Uncertainty flag (:) on (b-y) --- m1 colour mag u_m1 Uncertainty flag (:) on m1 --- c1 colour mag u_c1 Uncertainty flag (:) on c1 --- beta magnitude mag u_beta Uncertainty flag (:) on beta --- CDS 1993 May 18 J_A+A_275_484.xml Environment dependence of interstellar extinction curves J/A+A/275/549 J/A+A/275/549 Environment dependence of interstellar Environment dependence of interstellar extinction curves P Jenniskens J M Greenberg Astron. Astrophys. 275 549 1993 1993A&A...275..549J dust, extinction HII regions reflection nebulae ultraviolet: ISM The data are a decomposition of the extinction curves published by Aiello S., Barsella B., Chlewicki G., Greenberg J.M., Patriarchi P., and Perinotto M. (1988, A&A S 73, 195) in the parameter scheme of Fitzpatrick E.L. and Massa D. (1988, ApJ 328, 734). Each extinction curve k(x) = (A(lambda)-A(V))/(A(B)-A(V)) is given by: k(x) = c1 + c2*x + c3* D(x,x0,y) + c4*F(x) Where x = 1/wavelength (in inverse micron), D is a Drude profile: D(x,x0,y) = x^2/((x^2-x0^2)^2 + y^2x^2) and F is a polynomial of order 3: F(x) = 0.05392(x-5.9)^2 + 0.0564(x-5.9)^3 for 5.9<x<8.0 F(x) = 0 for x<5.9 In this scheme the parameters have the following meaning: c1: related directly to c2 because of normalisation k(x) c2: slope of the linear rise ( mag/E(B-V) ) y: width of the bump (inverse micron) c3: c3/y^2 is bump height, pi*c3/(2.*y) is bump area x0: position of the bump (inverse micron) c4: amount of FUV non-linear rise contribution: at 8 mu^-1: 2.9c4 (mag/E(B-V)) | * ^ | * 2.9c4 | ^ * * k(x)| c3/y^2 * * * .. v | *< y >* *.. | v * .. * * | *.. c2 1 | * 0 | * |^ * |Rv * |v____________________________|_____________________________ V B x0 5.9 8.0 x=1/wavelength (1/micron) Values of Rv, the ratio of total to selective extinction, can be found in Aiello et al. (1988).
Extinction coefficients starname Star Name --- k(U) Extinction in U band --- c1 Coefficient (see text) --- c2 Coefficient (see text) um c3 Coefficient (see text) --- c4 Coefficient (see text) --- y Width of the bump um-1 x0 Position of the bump um-1 CHISQ Indication of the deviation between fitted curve and actual data --- Q Quality indication of the data: Q=1 gives a bad fit to the U band extinction, f.e. due to saturation at long wavelength, and spectra marked Q=2 show signs of underexposure in the bump. --- IPSC IRAS point source classification: IPSC=1 is point source with 12 micron flux smaller than 25, IPSC=2 is point source with 25 micron flux smaller than 12. --- TYPE Environment characterisation from IRAS Skyflux maps CS: circumstellar DIF: diffuse medium line of sight (no aparent heating) BUB: bubble, extended region of increased 60/100 around OB association HII: HII region, compact regions of highly in creased 60/100 REF: reflection nebulae, small compact regions of highly increased 60/100 associated with B type stars. --- Patricia Bauer CDS 1993 Sep 10 J_A+A_275_549.xml The Velocity Field of the outer Galaxy J/A+A/275/67 J/A+A/275/67 The Velocity Field of the outer Galaxy The Velocity Field of the outer Galaxy J Brand L Blitz Astron. Astrophys. 275 67 1993 1993A&A...275...67B Galaxy: kinematics and dynamics Galaxy: structure *** No Description Available ***
Kinematically distinct complexes of optically visible HII regions -- (spectro-) photometric distances and radial velocities. Object Identification HII region S=Sharpless (ApJS 4, 257) BBW=Brand, Blitz & Wouterloot (A&AS 65, 537) . glon Galactic longitude deg glat Galactic latitude deg dist (Spectro-) photometric distance kpc e_dist Uncertainty in distance kpc Vlsr Velocity of the associated molecular gas km/s e_Vlsr Uncertainty in velocity km/s Assoc Associated HII regions . Jan Brand Bologna 1993 Feb 19 J_A+A_275_67.xml Compositional differences among the A-type stars. I. Six narrow lined stars. J/A+A/276/142 J/A+A/276/142 Compositional differences among the A-type stars. I. Compositional differences among the A-type stars. I. Six narrow lined stars. G M Hill J D Landstreet Astron. Astrophys. 276 142 1993 1993A&A...276..142H Abundances Stars, Ap stars: abundances stars: chemically peculiar stars: individual (omi Peg, Sirius) *** No Description Available ***
Line list for spectrum synthesis Id Element identification --- lambda Wavelength (A) 0.1nm log.gf log gf --- Ref Reference number=1 References: a: Kurucz (1989) b: Martin et al. (1988) c: Fuhr et al. (1988) d: Magazzu and Cowley (1986) e: Wiese et al. (1966) f: Kurucz & Peytremann (1975) g: Biemont et al. (1981) h: Wiese and Martin (1980) i: Ward (1985) j: Biemont et al. (1982) k: Sigut & Landstreet (1990) l: Younger et al. (1978) m: Lanz & Artru (1985) n: Hannaford et al. (1982) o: Wiese et al. (1969) p: Thevenin (1989) --- CDS 1993 Apr 14 J_A+A_276_142.xml Results of the ESO-SEST Key Programme on CO in the Magellanic Clouds. I. A survey of CO in the LMC and the SMC. J/A+A/276/25 J/A+A/276/25 Results of the ESO-SEST Key Programme on CO in the Results of the ESO-SEST Key Programme on CO in the Magellanic Clouds. I. A survey of CO in the LMC and the SMC. F P Israel L E B Johansson J Lequeux R S Booth L -A Nyman P Crane M Rubio T De Graauw M L Kutner R Gredel F Boulanger G Garay B Westerlund Astron. Astrophys. 276 25 1993 1993A&A...276...25I Interstellar medium Magellanic Clouds Radio lines galaxies: ISM ISM: clouds ISM: molecules Magellanic Clouds radio lines: galaxies *** No Description Available ***
(1-0) 12CO parameters LMC sources (1-0) 12CO parameters SMC sources Object LI-LMC(table1) or LI-SMC(table2) designation, IR nomenclature from Schwering 1989, Schwering & Israel 1989,1990 --- CO_flag Blended CO compomemts --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec l_T(mb) for upper limit --- T(mb) 12CO Line Parameter mK u_T(mb) uncertainty flag on T(mb) --- e_T(mb) rms uncertainty in T(mb) mK DeltaV 12CO Line Parameter km/s u_DeltaV uncertainty flag on DeltaV --- V(LSR)+ Velocity sign --- V(LSR) 12CO Line Parameter km/s u_V(LSR) uncertainty flag on V(LSR) --- I(CO) 12CO Line Parameter K.km/s u_I(CO) uncertainty flag on I(CO) --- Henize Henize name --- (1-0) 13CO parameters LMC sources (1-0) 13CO parameters SMC sources Object LI-LMC(table3) or LI-SMC(table4) --- RAh Right Ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec T(mb) 13CO Line Parameter mK e_T(mb) rms uncertainty on T(mb) mk DeltaV 13CO Line parameter km/s V(LSR) 13CO Line parameter km/s I(CO) 13CO Line parameter K.km/s I12/I13 Ratio I(12CO)/I(13CO) --- CDS 1993 Sep 15 J_A+A_276_25.xml The spectrum of FG Sge in 1992 J/A+A/276/389 J/A+A/276/389 The spectrum of FG Sge in 1992 The spectrum of FG Sge in 1992 T Kipper M Kipper Astron. Astrophys. 276 389 1993 1993A&A...276..389K Abundances stars: abundances stars: chemically peculiar Wavelength measurements and line identifications from the 0.14A/pixel echelle spectra of FG Sge secured two weeks before the drastic dimming of the star in 1992 are presented. The abundances of 18 elements are derived. These abundances have not changed from 1986. The main features of the chemical composition of FG Sge atmosphere are the depletion of iron-group elements and the marked overabundances (up to 3 dex) of s-process elements. First time in the observational history of FG Sge C_2_ Swan bands are identified in its spectrum.
FG Sge 20 11 55.8 +20 20 05
Line identifications in FG Sge LamObs Measured wavelength 0.1nm Rc Eye estimate of the residual intensity R_c_ multiplied by 10 --- Lam Identification wavelength 0.1nm Name Name of the line identified --- Patricia Bauer CDS 1996 Jan 10 J_A+A_276_389.xml An OH satellite line maser survey of cool IRAS sources and circumstellar envelope evolution J/A+A/277/453 J/A+A/277/453 OH maser survey of cool IRAS sources An OH satellite line maser survey of cool IRAS sources and circumstellar envelope evolution P David A M Le Squeren P Sivagnanam Astron. Astrophys. 277 453 1993 1993A&A...277..453D masers radio lines: circumstellar radio lines: molecular stars: evolution stars: mass-loss surveys *** No Description Available ***
Detected OH masers at 1612MHz Name IRAS name --- Class IRAS LRS class (blank when not available) --- GLON Galactic longitude deg GLAT Galactic latitude deg Flux(Vlow) Low velocity peak flux Jy n_Flux(Vlow) N when not measurable --- Flux(Vhigh) High velocity peak flux Jy n_Flux(Vhigh) N when not measurable --- Vlow Low velocity km/s n_Vlow N when not measurable --- Vhigh High velocity km/s n_Vhigh N when not measurable --- EVexp Envelope expansion velocity km/s n_EVexp N when not measurable --- Vr Stellar radial velocity km/s n_Vr N when not measurable --- Name OH name --- nRef Number of references --- Refs References (each reference is 4 bytes) --- Undetected sources at 1612MHz Name IRAS name --- Patricia Bauer CDS 1993 Oct 7 J_A+A_277_453.xml Automated identification of OB associations in M 31 J/A+A/278/36 J/A+A/278/36 M 31 new OB associations Automated identification of OB associations in M 31 E A Magnier P Battinelli W H G Lewin Z Haiman J Van Paradijs G Hasinger W Pietsch R Supper J Truemper Astron. Astrophys. 278 36 1993 1993A&A...278...36M II/208 : BVRI CCD photometry in the field of M 31 (Magnier+ 1992) Associations, stellar Positional data galaxies: individual (M 31) galaxies: spiral galaxies: star clusters methods: data analysis A new identification of OB associations in M 31 has been performed using the Path Linkage Criterion technique of Battinelli (1991A&A...244...69B). We found 174 associations with a very small contamination (<5%) by random clumps stars. The expected total number and average size of OB associations in the region of M 31 covered by our data set (Magnier et al., 1992, Cat. <II/208>) are ~280 and ~90pc, respectively. M 31 associations therefore have sizes similar to those of OB associations observed in nearby galaxies, so that we can consider them to be classical OB associations. This list of OB associations will be used for the study of the spatial distribution of OB associations and their correlation with other objects. Taking into account the fact that we do not cover the entire disk of M 31, we extrapolate a total number of associations in M 31 of ~420.
Associations in M 31 MLB93 OB association number --- RAdeg Right ascension (J2000.0) deg DEdeg Declination (J2000.0) deg Diam Clump diameter pc NStar Number of stars --- James Marcout, Patricia Bauer CDS 1997 Sep 26 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+A_278_36.xml X-ray Emission from a Complete Sample of Abell Clusters of Galaxies J/A+A/278/379 J/A+A/278/379 X-ray Emission from Abell Clusters of Galaxies X-ray Emission from a Complete Sample of Abell Clusters of Galaxies U G Briel J P Henry Astron. Astrophys. 278 379 1993 1993A&A...278..379B Clusters, galaxy X-ray sources cosmology: observations galaxies: clusters: general X-rays: galaxies The results of ROSAT All-Sky Survey (RASS, see cat. <IX/10>) have been used to investigate the X-ray properties of a complete sample of Abell clusters within a 561 square degree region at high galactic latitude; the mean redshift of the sample is 0.17.
Summary of the characteristics and X-ray results of the deep cluster sample Abell Abell Number --- RAh Right Ascension (1950) number=1 the position listed corresponds to the geometrical "average" position of those (frequently very few) galaxies listed by Huchra et al. (1990ApJ...365...66H) h RAm Right Ascension (1950) number=1 the position listed corresponds to the geometrical "average" position of those (frequently very few) galaxies listed by Huchra et al. (1990ApJ...365...66H) min RAs Right Ascension (1950) number=1 the position listed corresponds to the geometrical "average" position of those (frequently very few) galaxies listed by Huchra et al. (1990ApJ...365...66H) s DE- Declination sign number=1 the position listed corresponds to the geometrical "average" position of those (frequently very few) galaxies listed by Huchra et al. (1990ApJ...365...66H) --- DEd Declination (1950) number=1 the position listed corresponds to the geometrical "average" position of those (frequently very few) galaxies listed by Huchra et al. (1990ApJ...365...66H) deg DEm Declination (1950) number=1 the position listed corresponds to the geometrical "average" position of those (frequently very few) galaxies listed by Huchra et al. (1990ApJ...365...66H) arcmin DEs Declination (1950) number=1 the position listed corresponds to the geometrical "average" position of those (frequently very few) galaxies listed by Huchra et al. (1990ApJ...365...66H) arcsec z Redshift --- Rich. Abell's richness --- ACO ACO's galaxy counts --- N(HI) Galactic neutral hydrogen column density 10+21/cm2 FCCC Fraction of cluster counts collected --- Exp ROSAT-All-Sky-Survey exposure time s NCR Net counting rate ct/ks e_NCR 1-sigma error of the counting rate ct/ks l_XFlux limit flag on X-ray flux --- XFlux X-ray flux in 0.5-2.5 keV (observed frame) 10-16W/m2 l_XLum limit flag on X-ray luminosity --- XLum X-ray luminosity in 0.5-2.5 keV (rest frame) for H_o = 50 km/s/Mpc and q_o = 0.5 (unit 10+44 erg/s) 10+37W Patricia Bauer CDS 1993 Dec 22 Ulrich G. Briel <ugb@mpeu16.rosat.mpe-garching.mpg.de> UNKNOWN UNKNOWN * 22-Dec-1993: first archived as CDS * 21-Apr-1997: duplicated cluster A 1918 removed J_A+A_278_379.xml Spot and flare activity of FK Comae Berenices: long-term photometry J/A+A/278/449 J/A+A/278/449 Long-term photometry of FK Com Spot and flare activity of FK Comae Berenices: long-term photometry L Jetsu J Pelt I Tuominen Astron. Astrophys. 278 449 1993 1993A&A...278..449J stars: activity stars: flare stars: individual (FK Com) stars: variables: general *** No Description Available ***
Normalized photometry Year Average observing time yr Pphot Photometric rotation period d e_Pphot rms uncertainty on Pphot d Phi(min) Phase of the light minimum --- e_Phi(min) rms uncertainty on Phi(min) --- t_min Heliocentric julian date of the light minimum d Phi(tmin) Photometric phase --- Phi(coh) Coherence length --- e_Phi(coh) rms uncertainty on Phi(coh) --- SET Division into subset of the observing time --- Photometric phases of FK Comae flares HJD_flare Average time d Phi(flare) Photometric phase --- Delta Phase difference (Phi(flare) - Phi(min)) between the flare and the photometric minimum of the subset --- SET Division into subsets of the observing time --- F Category of the flare detection --- Mean brightness in UBVRI YEAR Average observing time yr M(U) Mean brightness in U filter mag e_M(U) rms uncertainty on M(U) mag M(B) Mean brightness in B filter mag e_M(B) rms uncertainty on M(B) mag M(V) Mean brightness in V filter mag e_M(V) rms uncertainty on M(V) mag M(R) Mean brightness in R filter mag e_M(R) rms uncertainty on M(R) mag M(I) Mean brightness in I filter mag e_M(I) rms uncertainty on M(I) mag SET Division into subsets of the observing time --- Amplitude of the rotational modulation of brightness in UBVRI YEAR Average observing time yr A(U) Amplitude of the rotational modulation of brightness in U filter --- e_A(U) rms uncertainty on A(U) --- A(B) Amplitude of the rotational modulation of brightness in B filter --- e_A(B) rms uncertainty on A(B) --- A(V) Amplitude of the rotational modulation of brightness in V filter --- e_A(V) rms uncertainty on A(V) --- A(R) Amplitude of the rotational modulation of brightness in R filter --- e_A(R) rms uncertainty on A(R) --- A(I) Amplitude of the rotational modulation of brightness in I filter --- e_A(I) rms uncertainty on A(I) --- SET Division into subset of observing time --- Patricia Bauer CDS 1993 Oct 28 J_A+A_278_449.xml The relation between BL Lac objects and OVV quasars, and the unified model of BL Lac objects, FR-I and FR-II(G) radio galaxies J/A+A/278/6 J/A+A/278/6 BL Lac objects and OVV quasars The relation between BL Lac objects and OVV quasars, and the unified model of BL Lac objects, FR-I and FR-II(G) radio galaxies G Z Xie Y H Zhang J H Fan F K Liu Astron. Astrophys. 278 6 1993 1993A&A...278....6X BL Lacertae objects: general galaxies: active quasars: general *** No Description Available ***
X-ray selected BL Lac objects Radio selected BL Lac objects Note If (*) or (@); BL Lac objects discussed in previous paper (Xie et al., 1991) --- Designation Coordinate designation (1950) --- Name Name --- m(min) Faintest apparent V magnitude mag r_m See note number=1 References to table 1,2 1. Maccacaro et al. 1989 2. Stocke et al. 1990a 3. Stocke et al. 1990b 4. Taglicaferri et al. 1989 5. Piccinotti et al. 1982 6. Remillard et al. 1989 7. Giommi et al. 1987 8. Veron-Cetty et al. 1987 9. Burbidge et al. 1987 10.Urry 1984 11.Stocke et al. 1985 12.Moles et al. 1985 13.Bassani et al. 1983 14.Spinead et al. 1975 15.Xie et al. 1990 16.Filippenko et al. 1986 17.Preston et al. 1985 18.Smith et al 1987 19.Impey et al. 1988 20.Miller 1975 21.Bolton et al. 1968 22.Stocke et al. 1983 23.Brindle et al. 1986 24.Xie et al. 1989 25.Feigelson et al. 1986 26.Doxsey et al. 1983 27.Treves et al. 1986 28.Xie et al. 1988a 29.Xie et al. 1988b 30.Maraschi et al. 1986 31.Impey et al. 1982 32.Stick et al. 1988 33.Allen et al. 1982 34.Carrasco et al. 1985 35.Valtaoja et al. 1985 36.Xie et al. 1991c 37.Chisellini et al. 1986 38.Arp et al. 1979 39.Persic et al. 1984 40.Wing 1973 41.Stickel et al. 1991 42.Giacani et al. 1988 43.Smith et al. 1987 44.Craine 1977 45.Impey et al. 1984 46.Burbidge et al. 1989 47.Ledden et al. 1985 48.Hewitt et al 1987 49.Kuhr et al. 1990 50.Smith et al 1987 51.Golombek 1988 52.Xie et al. 1992 53.Schalinski 1987 54.Angione et al 1971 55.Baldes et al. 1980 56.Staubert et al. 1986 57.Stein et al. 1976 --- Z Redshift --- r_Z See note number=1 References to table 1,2 1. Maccacaro et al. 1989 2. Stocke et al. 1990a 3. Stocke et al. 1990b 4. Taglicaferri et al. 1989 5. Piccinotti et al. 1982 6. Remillard et al. 1989 7. Giommi et al. 1987 8. Veron-Cetty et al. 1987 9. Burbidge et al. 1987 10.Urry 1984 11.Stocke et al. 1985 12.Moles et al. 1985 13.Bassani et al. 1983 14.Spinead et al. 1975 15.Xie et al. 1990 16.Filippenko et al. 1986 17.Preston et al. 1985 18.Smith et al 1987 19.Impey et al. 1988 20.Miller 1975 21.Bolton et al. 1968 22.Stocke et al. 1983 23.Brindle et al. 1986 24.Xie et al. 1989 25.Feigelson et al. 1986 26.Doxsey et al. 1983 27.Treves et al. 1986 28.Xie et al. 1988a 29.Xie et al. 1988b 30.Maraschi et al. 1986 31.Impey et al. 1982 32.Stick et al. 1988 33.Allen et al. 1982 34.Carrasco et al. 1985 35.Valtaoja et al. 1985 36.Xie et al. 1991c 37.Chisellini et al. 1986 38.Arp et al. 1979 39.Persic et al. 1984 40.Wing 1973 41.Stickel et al. 1991 42.Giacani et al. 1988 43.Smith et al. 1987 44.Craine 1977 45.Impey et al. 1984 46.Burbidge et al. 1989 47.Ledden et al. 1985 48.Hewitt et al 1987 49.Kuhr et al. 1990 50.Smith et al 1987 51.Golombek 1988 52.Xie et al. 1992 53.Schalinski 1987 54.Angione et al 1971 55.Baldes et al. 1980 56.Staubert et al. 1986 57.Stein et al. 1976 --- log(L) Bolometric luminosity 10-7W r_log(L) See note number=1 References to table 1,2 1. Maccacaro et al. 1989 2. Stocke et al. 1990a 3. Stocke et al. 1990b 4. Taglicaferri et al. 1989 5. Piccinotti et al. 1982 6. Remillard et al. 1989 7. Giommi et al. 1987 8. Veron-Cetty et al. 1987 9. Burbidge et al. 1987 10.Urry 1984 11.Stocke et al. 1985 12.Moles et al. 1985 13.Bassani et al. 1983 14.Spinead et al. 1975 15.Xie et al. 1990 16.Filippenko et al. 1986 17.Preston et al. 1985 18.Smith et al 1987 19.Impey et al. 1988 20.Miller 1975 21.Bolton et al. 1968 22.Stocke et al. 1983 23.Brindle et al. 1986 24.Xie et al. 1989 25.Feigelson et al. 1986 26.Doxsey et al. 1983 27.Treves et al. 1986 28.Xie et al. 1988a 29.Xie et al. 1988b 30.Maraschi et al. 1986 31.Impey et al. 1982 32.Stick et al. 1988 33.Allen et al. 1982 34.Carrasco et al. 1985 35.Valtaoja et al. 1985 36.Xie et al. 1991c 37.Chisellini et al. 1986 38.Arp et al. 1979 39.Persic et al. 1984 40.Wing 1973 41.Stickel et al. 1991 42.Giacani et al. 1988 43.Smith et al. 1987 44.Craine 1977 45.Impey et al. 1984 46.Burbidge et al. 1989 47.Ledden et al. 1985 48.Hewitt et al 1987 49.Kuhr et al. 1990 50.Smith et al 1987 51.Golombek 1988 52.Xie et al. 1992 53.Schalinski 1987 54.Angione et al 1971 55.Baldes et al. 1980 56.Staubert et al. 1986 57.Stein et al. 1976 --- log[Delta(t_min)] Minimum variability timescale Delta(t_min) s r_Delta(t_min) See note number=1 References to table 1,2 1. Maccacaro et al. 1989 2. Stocke et al. 1990a 3. Stocke et al. 1990b 4. Taglicaferri et al. 1989 5. Piccinotti et al. 1982 6. Remillard et al. 1989 7. Giommi et al. 1987 8. Veron-Cetty et al. 1987 9. Burbidge et al. 1987 10.Urry 1984 11.Stocke et al. 1985 12.Moles et al. 1985 13.Bassani et al. 1983 14.Spinead et al. 1975 15.Xie et al. 1990 16.Filippenko et al. 1986 17.Preston et al. 1985 18.Smith et al 1987 19.Impey et al. 1988 20.Miller 1975 21.Bolton et al. 1968 22.Stocke et al. 1983 23.Brindle et al. 1986 24.Xie et al. 1989 25.Feigelson et al. 1986 26.Doxsey et al. 1983 27.Treves et al. 1986 28.Xie et al. 1988a 29.Xie et al. 1988b 30.Maraschi et al. 1986 31.Impey et al. 1982 32.Stick et al. 1988 33.Allen et al. 1982 34.Carrasco et al. 1985 35.Valtaoja et al. 1985 36.Xie et al. 1991c 37.Chisellini et al. 1986 38.Arp et al. 1979 39.Persic et al. 1984 40.Wing 1973 41.Stickel et al. 1991 42.Giacani et al. 1988 43.Smith et al. 1987 44.Craine 1977 45.Impey et al. 1984 46.Burbidge et al. 1989 47.Ledden et al. 1985 48.Hewitt et al 1987 49.Kuhr et al. 1990 50.Smith et al 1987 51.Golombek 1988 52.Xie et al. 1992 53.Schalinski 1987 54.Angione et al 1971 55.Baldes et al. 1980 56.Staubert et al. 1986 57.Stein et al. 1976 --- alpha Optical spectral index alpha --- r_alpha See note number=1 References to table 1,2 1. Maccacaro et al. 1989 2. Stocke et al. 1990a 3. Stocke et al. 1990b 4. Taglicaferri et al. 1989 5. Piccinotti et al. 1982 6. Remillard et al. 1989 7. Giommi et al. 1987 8. Veron-Cetty et al. 1987 9. Burbidge et al. 1987 10.Urry 1984 11.Stocke et al. 1985 12.Moles et al. 1985 13.Bassani et al. 1983 14.Spinead et al. 1975 15.Xie et al. 1990 16.Filippenko et al. 1986 17.Preston et al. 1985 18.Smith et al 1987 19.Impey et al. 1988 20.Miller 1975 21.Bolton et al. 1968 22.Stocke et al. 1983 23.Brindle et al. 1986 24.Xie et al. 1989 25.Feigelson et al. 1986 26.Doxsey et al. 1983 27.Treves et al. 1986 28.Xie et al. 1988a 29.Xie et al. 1988b 30.Maraschi et al. 1986 31.Impey et al. 1982 32.Stick et al. 1988 33.Allen et al. 1982 34.Carrasco et al. 1985 35.Valtaoja et al. 1985 36.Xie et al. 1991c 37.Chisellini et al. 1986 38.Arp et al. 1979 39.Persic et al. 1984 40.Wing 1973 41.Stickel et al. 1991 42.Giacani et al. 1988 43.Smith et al. 1987 44.Craine 1977 45.Impey et al. 1984 46.Burbidge et al. 1989 47.Ledden et al. 1985 48.Hewitt et al 1987 49.Kuhr et al. 1990 50.Smith et al 1987 51.Golombek 1988 52.Xie et al. 1992 53.Schalinski 1987 54.Angione et al 1971 55.Baldes et al. 1980 56.Staubert et al. 1986 57.Stein et al. 1976 --- eta(ob) Efficiency of the conversion of accreted matter into energy --- delta Doppler factor delta --- m(corr) Corrected apparent magnitude min Sample of OVV quasars Designation Coordinate designation (1950) --- Name Name --- V(min) Faintest apparent V magnitude mag Z Redshift --- Sample of FR-I radio galaxies Sample of FR-II(G) radio galaxies Sample of FR-II(Q) radio galaxies Designation Coordinate designation (1950) --- Name Name --- V Apparent V magnitude mag Z Redshift --- u_Z Uncertaincy flag on redshift --- Patricia Bauer CDS 1993 Sep 30 J_A+A_278_6.xml Submillimeter observations of the shocked molecular gas associated with the supernova remnant IC 443 J/A+A/279/541 J/A+A/279/541 Submillimeter obs of shocked molecular Submillimeter observations of the shocked molecular gas associated with the supernova remnant IC 443 E F Van Dishoeck D J Jansen T G Phillips Astron. Astrophys. 279 541 1993 1993A&A...279..541V ISM: individual (IC 443) ISM: molecules radio lines: ISM shock waves supernova remnants Submillimeter observations of various simple molecules in the shocked molecular gas associated with the supernova remnant IC 443 are presented. CO 3-2 line profiles along the shocked ring are used to constrain the global kinematics of the region. Searches for other molecules in the shocked gas have been performed at two positions in clump G and one position in clump B. High-frequency lines of HCO(+), HCN, HNC, CS, SO, SiO, H2CO and C2H have been detected, and significant upper limits have been obtained for various other, more complex molecules. The physical parameters in the shocked gas have been derived from an analysis of the excitation of these species. The observed abundances are substantially lower than those found in one-fluid hydrodynamic shock models with a small H/H2 ratio, but appear consistent with the limited models in which H/H2 is significant.
Observations and fits of IC 443 G I Observations and fits of IC 443 G II Observations and fits of IC 443 B Species Ion or molecule name --- Transit Transition levels upper-lower --- Freq Frequency MHz l_T(MB) '<' if T(MB) is an upper limit (upper limits are 2 sigma values in 1 MHz bandwidth) --- T(MB) Main beam temperature K V(LSR) Velocity km/s DV FWHM of line km/s W Main beam temperature integrated over profile K.km/s Note Remark (see below) --- Obs Telescope and Year of observation --- Francois Ochsenbein CDS 1993 Jul 20 J_A+A_279_541.xml Abundances of non-type I planetary nebulae in the LMC J/A+A/279/567 J/A+A/279/567 Abundances of non-type I planetary nebulae in the Abundances of non-type I planetary nebulae in the LMC J A Freitas Pacheco R D D Costa W J Maciel Astron. Astrophys. 279 567 1993 1993A&A...279..567D galaxies: abundances Magellanic Clouds planetary nebulae: general Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.
Line intensities for the nebulae Name SMP denomination of the nebula --- n_I When blank, observed fluxes, when c, extinction-corrected fluxes --- I4340 Hgamma line intensity (scale F(Hbeta)=100) --- u_I4340 uncertainty flag on I4340 --- I4363 line intensity (scale F(Hbeta)=100) --- u_I4363 uncertainty flag on I4363 --- I4686 HeII line intensity (scale F(Hbeta)=100) --- I4861 Hbeta line intensity --- I5007 line intensity (scale F(Hbeta)=100) --- I5411 HeII line intensity (scale F(Hbeta)=100) --- I5754 line intensity (scale F(Hbeta)=100) --- u_I5754 uncertainty flag on I5754 --- I5876 HeI line intensity (scale F(Hbeta)=100) --- I6300 line intensity (scale F(Hbeta)=100) --- I6312 line intensity (scale F(Hbeta)=100) --- I6563 Halpha line intensity (scale F(Hbeta)=100) --- I6584 line intensity (scale F(Hbeta)=100) --- I6678 HeI line intensity (scale F(Hbeta)=100) --- I6724 line intensity (scale F(Hbeta)=100) --- I7005 line intensity (scale F(Hbeta)=100) --- I7065 HeI line intensity (scale F(Hbeta)=100) --- I7135 line intensity (scale F(Hbeta)=100) --- I7325 line intensity (scale F(Hbeta)=100) --- R(SII) R(SII) --- E(B-V) E(B-V) --- Physical properties Object SMP denomination of the nebula --- T(OIII) OIII temperature K u_T(OIII) uncertainty flag on T(OIII) K r_T(OIII) References to T(OIII) number=2 References: 1: Aller, L.H., Keyes, C.D., Maran, S.P., Gull, T.R., Michalitsianos, A.G., Stecher, T,P. 1987, ApJ 320, 159 2: Henry, R.B.C., Liebert, J., Boronson, T.A. 1989, ApJ 339, 872 3: Meatheringham, S.J. & Dopita, M.A. 1991 ApJSS 76, 1085 4: Monk, D.J., Barlow, M.J., Clegg, R.E.S. 1988, MNRAS 234, 583 5: Vassiliadis, E., Dopita, M.A., Morgan, D.A., Bell, J.F. 1992, ApJSS 83, 87 K T(NII) NII temperature K u_T(NII) uncertainty flag on T(NII) K ne Electronic number cm-3 Elemental abundances Name SMP denomination of the nebula --- He/H He/H abundance --- Ab(O) O abundance in the scale log(O/H) + 12 --- Ab(N) N abundance in the scale log(N/H) + 12 --- Ab(S) S abundance in the scale log(S/H) + 12 --- Ab(Ar) Ar abundance in the scale log(Ar/H) + 12 --- Oxygen abundances in the LMC Object Object type --- Ab(O) O abundance in the scale log(O/H) + 12 --- e_Ab(O) rms uncertainty on Ab(O) --- Source Source --- Patricia Bauer CDS 1993 Jul 26 J_A+A_279_567.xml The extinction and star clusters in NGC 1275 J/A+A/279/61 J/A+A/279/61 extinction and star clusters in NGC 1275 The extinction and star clusters in NGC 1275 H U Norgaard-Nielsen P Goudfrooij H E Jorgensen L Hansen Astron. Astrophys. 279 61 1993 1993A&A...279...61N galaxies: cooling flows galaxies: individual (NGC 1275) galaxies: interactions galaxies: ISM galaxies: star clusters Our CCD images reveal that some of the well-known absorption features in NGC 1275 do not show up in the distribution of the low velocity (LV) ionized gas. The absorption features have the same asymmetrical distribution around the nucleus as the high velocity (HV) emission line system. The extinction of the features is significantly different from the Galactic law. Our analysis shows that the dust responsible for the extinction is most probably well within NGC 1275. Altogether, we argue that most of the absorption features are associated with the HV system, implying that the HV system has moved halfway through NGC 1275. We have found many more objects than recently discovered by Hubble Space Telescope (HST)(Holtzman et al. 1992). We have been able to define three groups of objects with distinct differences in distribution around the nucleus: (1) a group of mainly giant H II regions, nearly all associated with the HV system, (2) old globular clusters in a total number of about 2/3 of the number of globular clusters in M87 (assuming a universal luminosity function of globular clusters), and (3) an intermediate group (IG), of both extended and point sources, with 0.0 less than or equal to (V-I)(sub 0) less than or equal to 0.75. The IG is peaking strongly at the nucleus of NGC 1275, with a smooth and symmetrical distribution. For the extended IG objects, we estimate an age less than or equal to 10(exp 7) yr, while the point sources could have ages 10(exp 7) to 10(exp 9) yr. We suggest that the IG objects have been formed in a cooling catastrophe, set up in the central part of the extended X-ray emitting gas of the Perseus Cluster. Very little (except for the giant H II regions) excess light in our V frame can be associated with the HV system. We find -16.1 greater than or equal to M(sub V)(HV) greater than or equal to -17.3, implying that the HV system is extremely luminous in hydrogen alpha compared to the visual luminosity.
The excess objects in the residual V frame Object When starting with H, object observed by Holtzman et al. (1992) When starting with N, new object --- D_RA offset in right ascension from the nucleus arcsec D_DE offset in declination from the nucleus. The coordinate system of Holtzman et al. is rotated 2 deg NE arcsec V0 magnitude, corrected for Galactic extinction Av = 0.54 mag e_V0 photon noise in the V magnitude mag (V-I)0 color corrected for Galactic extinction E(V-I) = 0.28 mag e_(V-I)0 photon noise in (V-I)0 mag V0,H magnitude by Holztamn et al. corrected for Galactic extinction Av mag e_V0,H photon noise in the V0 magnitude mag (V-R)0 color by Holtzman et al. corrected for Galactic extinction E(V-R) = 0.14 mag e_(V-R)0 photon noise in (V-R)0 mag LV When +, the object is associated with a LV Halpha emission knot --- HV When +, the object is associated with a LV Halpha emission knot when ?, the object could be associated with HV Halpha emission knot --- group 1: old globular clusters 2: intermediate group objects 3: giant H II regions 4: foreground stars --- Comments Holtzman et al. objects included in our diaphragm. extended: object classified as diffuse by Holtzman et al. --- Patricia Bauer CDS 1993 Oct 27 J_A+A_279_61.xml H-alpha Survey of the Small Magellanic Cloud J/A+A/280/365 J/A+A/280/365 H-alpha Survey of SMC H-alpha Survey of the Small Magellanic Cloud E Le Coarer M Rosado Y Georgelin A Viale G Goldes Astron. Astrophys. 280 365 1993 1993A&A...280..365L galaxies: Magellanic Clouds galaxies: kinematics galaxies: ISM HII regions *** No Description Available ***
Velocities and H-alpha fluxes DEM Number in DEM catalogue (Davies R.D., Elliot K.H., Meaburn J., 1976, MNRAS 81, 89) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Vhel Heliocentric radial velocity of the nebular components km/s Disp Velocity dispersion (corrected only for the instrumental function) km/s Disp2 Velocity dispersions of other components km/s Diam Diaphram diameter arcmin Flux in H-alpha (10-10 erg/cm2/s) 10-13W/m2 Comment Comments as a plain text. --- Francois Ochsenbein CDS 1993 Dec 14 J_A+A_280_365.xml Chemical behaviour of planetary nebulae and galactic abundance gradients J/A+A/280/581 J/A+A/280/581 Chemical behaviour of planetary nebulae and gal Chemical behaviour of planetary nebulae and galactic abundance gradients A Pasquali M Perinotto Astron. Astrophys. 280 581 1993 1993A&A...280..581P Abundances Interstellar medium Nebulae, planetary Galaxy: abundances ISM: abundances planetary nebulae: general *** No Description Available ***
Chemical abundances of the PNe not included in Table 1 of Perinotto (1991) Planetary Nebulae of type I Planetary Nebulae of type IV Name Name of PNe --- PK PK number of PNe --- l_He/H Limit flag on He/H --- He/H Helium abundances with respect to H --- u_He/H Uncertainty flag on He/H --- O/H Oxygen abundances with respect to H, 10-4 u_O/H Uncertainty flag on O/H --- l_N/O Limit flag on N/O --- C/O Carbon abundances with respect to Oxygen --- u_C/O Uncertainty flag on C/O --- l_N/O Limit flag on N/O --- N/O Nytrogen abundances with respect to Oxygen --- u_N/O Uncertainty flag on N/O --- Ne/O Neon abundances with respect to Oxygen --- u_Ne/O Uncertainty flag on Ne/O --- Sources References in literature. --- Z Z distances from the Galactic Plane calculated from Cahn et al. (1992) pc V(LSR) Radial velocities from Schneider et al. (1983) km/s Distances and velocities of PNe with known chemical abundances Name Name of PNe --- PK PK number of PNe --- Distance Distance calculated from Cahn et al. (1992) pc V(LSR) Radial velocities Schneider et al. (1983) km/s Francois Ochsenbein CDS 1993 Jul 26 J_A+A_280_581.xml The asymmetries in radio source structures. I. A comparison of two classical models. J/A+A/281/15 J/A+A/281/15 The asymmetries in radio source structures. I. The asymmetries in radio source structures. I. A comparison of two classical models. S Rys Astron. Astrophys. 281 15 1994 1994A&A...281...15R galaxies: active quasars: general radio continuum: galaxies A method is suggested for the mathematical description of the asymmetry occurring in the radio-source structures. The method is based on the transformation of the radio structure into 'itself' and may be used for all morphological types of structures. Two models of generation of the source asymmetry are investigated, namely Doppler effects and the flip-flop mechanism, with an assumption that the luminosity of the plasma volume depends on time as a power law S approximately t(exp mu). The model with Doppler effects turns out to be more suitable than that with flip-flop mechanism.
The data sample Name IAU source name --- Id optical identification --- V optical magnitude mag Ftot total flux at 1.4 GHz (in radio map) Jy alf spectral index (power law: freq**(-alf)) --- LAS largest angular size arcsec MC number of map components --- The best fitting parameters for the models Name IAU source name --- Index1 index of shining rate number=1 parameters for Doppler model (fitted position) --- Vx1/c component of expansion velocity in the observer direction number=1 parameters for Doppler model (fitted position) --- INC1 flux incorrectness (for the best fit case) number=1 parameters for Doppler model (fitted position) % inc1 shape incorrectness (for the best fit case)(1) % Index2 index of shining rate number=2 parameters for Doppler model (fixed position) --- Vx2/c component of the expansion velocity in the observer direction number=2 parameters for Doppler model (fixed position) --- INC2 flux incorrectness (for the best fit case)(2) % inc2 shape incorrectness (for the best fit case)(2) % Index3 index of shining rate number=3 parameters for Flip-flop model (fitted position) --- B3 difference in twins positions number=3 parameters for Flip-flop model (fitted position) % INC3 flux incorrectness (for the best fit case)(3) % inc3 shape incorrectness (for the best fit case)(3) % Index4 index of shining rate number=4 parameters for Flip-flop model (fixed position) --- B4 difference in twins positions number=4 parameters for Flip-flop model (fixed position) % INC4 flux incorrectness (for the best fit case)(4) % inc4 shape incorrectness (for the best fit case)(4) % Patricia Bauer CDS 1993 Oct 12 J_A+A_281_15.xml Radio emission from stars: a survey at 250 GHz J/A+A/281/161 J/A+A/281/161 Radio emission from stars: a survey at 250 GHz Radio emission from stars: a survey at 250 GHz W J Altenhoff C Thum H J Wendker Astron. Astrophys. 281 161 1994 1994A&A...281..161A giants radio stars stars: pre-main sequence stars: variables: general stars: Wolf-Rayet stellar wind supergiants *** No Description Available ***
O and B stars WR stars Early-type stars with shells Name Star name (VCLS number for table5) --- l_S(250) Limit flag on S(250) --- S(250) Flux mJy e_S(250) rms uncertainty on S(250) mJy Session Number of sessions --- l_alf Limit flag on spectral index alf --- alf Spectral index --- e_alf rms uncertainty on spectral index --- u_alf uncertainty flag on spectral index --- Remarks Remarks --- Pre-main sequence stars Name Star name --- l_S(250) Limit flag on S(250) --- S(250) Flux mJy e_S(250) rms uncertainty on S(250) mJy Session Number of sessions --- l_alf Limit flag on spectral index alf --- alf Spectral index --- e_alf rms uncertainty on spectral index --- Remarks Remarks --- Stellar disks (giants and supergiants) Name Star name --- SpT Spectral type --- l_S(250) Limit flag on S(250) --- S(250) Flux mJy e_S(250) rms uncertainty on S(250) mJy Session Number of sessions --- l_alf Limit flag on spectral index --- alf Spectral index --- e_alf rms uncertainty on spectral index --- Remarks Remarks --- Stars with optically determined radii Name Star name number= (1) Mozurkewich et al. 1991 (2) di Benedetto & Rabbia 1987 (3) Hutter et al. 1989 (4) see text (5) Fracassini et al. 1981 (6) Hanbury Brown et al. 1974 (7) di Benedetto & Foy 1986 (8) Christou & Worden 1980 (9) di Benedetto & Ferluga 1990 --- Sp Spectral type number= (1) Mozurkewich et al. 1991 (2) di Benedetto & Rabbia 1987 (3) Hutter et al. 1989 (4) see text (5) Fracassini et al. 1981 (6) Hanbury Brown et al. 1974 (7) di Benedetto & Foy 1986 (8) Christou & Worden 1980 (9) di Benedetto & Ferluga 1990 --- R(UD) Stellar radius number= (1) Mozurkewich et al. 1991 (2) di Benedetto & Rabbia 1987 (3) Hutter et al. 1989 (4) see text (5) Fracassini et al. 1981 (6) Hanbury Brown et al. 1974 (7) di Benedetto & Foy 1986 (8) Christou & Worden 1980 (9) di Benedetto & Ferluga 1990 mas Ref. References --- l_S(250) Limit flag on S(250) number= (1) Mozurkewich et al. 1991 (2) di Benedetto & Rabbia 1987 (3) Hutter et al. 1989 (4) see text (5) Fracassini et al. 1981 (6) Hanbury Brown et al. 1974 (7) di Benedetto & Foy 1986 (8) Christou & Worden 1980 (9) di Benedetto & Ferluga 1990 --- S(250) Flux number= (1) Mozurkewich et al. 1991 (2) di Benedetto & Rabbia 1987 (3) Hutter et al. 1989 (4) see text (5) Fracassini et al. 1981 (6) Hanbury Brown et al. 1974 (7) di Benedetto & Foy 1986 (8) Christou & Worden 1980 (9) di Benedetto & Ferluga 1990 mJy l_T(disk) Limit flag on disk temperature number= (1) Mozurkewich et al. 1991 (2) di Benedetto & Rabbia 1987 (3) Hutter et al. 1989 (4) see text (5) Fracassini et al. 1981 (6) Hanbury Brown et al. 1974 (7) di Benedetto & Foy 1986 (8) Christou & Worden 1980 (9) di Benedetto & Ferluga 1990 --- T(disk) Disk temperature number= (1) Mozurkewich et al. 1991 (2) di Benedetto & Rabbia 1987 (3) Hutter et al. 1989 (4) see text (5) Fracassini et al. 1981 (6) Hanbury Brown et al. 1974 (7) di Benedetto & Foy 1986 (8) Christou & Worden 1980 (9) di Benedetto & Ferluga 1990 K Variable stars Name Star name --- Session Number of sessions --- l_S(250) limit flag on S(250) --- S(250) Flux mJy e_S(250) rms uncertainty on S(250) mJy Remarks Remarks --- Patricia Bauer CDS 1993 Oct 14 J_A+A_281_161.xml The X-ray AGN content of the Molonglo 408 MHz survey: bulk properties of previously optically identified sources. J/A+A/281/355 J/A+A/281/355 The X-ray AGN content of the Molonglo 408 MHz The X-ray AGN content of the Molonglo 408 MHz survey: bulk properties of previously optically identified sources. W Brinkmann J Siebert T Boller Astron. Astrophys. 281 355 1994 1994A&A...281..355B galaxies: active quasars: general radio continuum: galaxies X-rays: galaxies *** No Description Available ***
MRC-ROSAT sources with identifications MRC MRC identification --- Flux 408 MHz flux Jy Type Morphology flag number=1 Morphology flags: A: Small scale structure present E: Extended source (> 10 arcmin) C: Complex extended source M: Multiple sources (within 8 arcmin) N: Weak neighbouring sources --- Ref Cross-reference flag number=2 Cross-references flags: J: Source imaged at 843 MHz by Jones (1989) P: Source lies within 2 arcmin of a Parkes source S: Source in Schilizzi & McAdam (1975) M: Source in Clarke et al. (1976) C: Source in Cameron (1971) R: Source in Robertson (1973) T: A note exists in MRC original text (MNRAS 194, p. 696) --- Type Type of optical counterpart with some further specifications about its nature --- Mv Optical magnitude mag l_Z limit flag on redshift --- Z Redshift --- Name Common name of the source --- Rosat Rosat designation --- D Offset between X-ray and MRC radio position arcsec Flux X-ray flux mW/m2 e_Flux Error for the X-ray flux mW/m2 Patricia Bauer CDS 1993 Oct 13 J_A+A_281_355.xml Structures of small size radio galaxies in clusters J/A+A/281/375 J/A+A/281/375 Structures of small size radio galaxies Structures of small size radio galaxies in clusters L Feretti G Giovannini Astron. Astrophys. 281 375 1994 1994A&A...281..375F galaxies: clusters: general galaxies: ISM radio continuum: galaxies *** No Description Available ***
List of sources and their properties Clus Cluster name --- Name Radio source name --- Other Other radio galaxy name --- RAh Right ascension B1950 h RAm Right ascension B1950 min RAs Right ascension B1950 s DEd Declination B1950 deg DEm Declination B1950 arcmin DEs Declination B1950 arcsec z Cluster redshift --- Opt Galaxy optical type --- Ref Reference --- Observational data Clus Cluster name --- Name Radio source name --- Array VLA Configurations --- Time Observing time min Noise Map noise mJy BE1 FWHM of the beam major axis arcsec BE2 FWHM of the beam minor axis arcsec BEpa ]-90/+90[? Position angle of the beam major axis deg Radio parameters of the galaxies Clus Cluster name --- Name Radio source name --- l_Flux Limit flag on Flux --- Flux Flux density. mJy AS Angular size arcsec logP Logarithm of radio power at 1.4 GHz W/Hz l_Size Limit flag on Size --- Size Linear size. kpc umin Minimum energy density (10**-11 erg/cm3) pJ/m3 Struct Radio structure: D = double E = Extended-diffuse J = core-jet P = point-like T = tailed --- Radio galaxies belonging to the present sample, observed by other authors Clus Cluster name --- Name Radio source name --- Other Other radio galaxy name --- Flux Flux density at 1.4 GHz mJy AS Angular size arcsec LogP Logarithm of radio power at 1.4 GHz W/Hz Size Linear size at 1.4 GHz kpc Struct Radio structure --- Ref Reference --- Patricia Bauer CDS 1993 Oct 18 J_A+A_281_375.xml The chemical composition of the s-Cepheids: I. Alpha Ursae Minoris (Polaris) and HR 7308 (V473 Lyr): unique Cepheids of the Galaxy J/A+A/281/465 J/A+A/281/465 The chemical composition of the s-Cepheids: I. The chemical composition of the s-Cepheids: I. Alpha Ursae Minoris (Polaris) and HR 7308 (V473 Lyr): unique Cepheids of the Galaxy S M Andrievsky V V Kovtyukh I A Usenko Astron. Astrophys. 281 465 1994 1994A&A...281..465A Cepheids chemical composition s-Cepheids *** No Description Available ***
Observational data Name Star name --- Date Date "jj-mm-yy" HDJ Julian day d Phase Phase --- n_Phase Phases calculated according to: 1: Arellano Ferro (1984) 2: Eggen (1985) --- Emulsion Emulsion --- Region Ragion 0.1nm Exp. Exposure time min S/N Signal-to-noise ratio --- Residual intensities for hydrogen line profiles Delta(Lambda) Delta (Lambda) 0.1nm Hbeta Residual intensity for hydrogen line profile of Alpha UMi --- Hgamma Residual intensity for hydrogen line profile of Alpha UMi --- Hbeta Residual intensity for hydrogen line profile of HR7308(1990) --- Hgamma Residual intensity for hydrogen line profile of HR7308(1990) --- Hdelta Residual intensity for hydrogen line profile of HR7308(1990) --- Hgamma Residual intensity for hydrogen line profile of HR7308(1992) --- Hdelta Residual intensity for hydrogen line profile of HR7308(1992) --- Chemical composition of Aplha UMi Element Element number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 --- NL Line number used for this study number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 --- (E/H) Mean abundance relative to logN(H) = 12 the mean abundance is relative to logN(H) = 12 number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 --- [E/H] (E/H) with respect to solar values number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun e_[E/H] rms uncertainty on [E/H] number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun B&L [E/H] Boyarchuck & Luybimkov (1991b) result number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun L&B [E/H] Luck & Bond (1986) result number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun GIR [E/H] Giridhar (1985) result number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun SR&J [E/H] Sanwal, Rautela & Joshi (1988) result number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun Chemical composition of HR7308 Element Element number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 --- NL Line number used for the 1990 value number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 --- (E/H) Mean abundance, 1990 value the mean abundance is relative to logN(H) = 12 --- [E/H] (E/H) with respect to solar value, 1990 value number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun e_[E/H] rms uncertainty on [E/H], 1990 value number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun NL Line number used for average 1992 value number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 --- (E/H) Mean abundance, average 1992 value the mean abundance is relative to logN(H) = 12 --- [E/H] (E/H) with respect to solar value, average 1992 value number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun e_[E/H] rms uncertainty on [E/H], average 1992 value number= In abundances determination the hyper-fine structure was not taken into account. number= the mean abundance is relative to logN(H) = 12 Sun Equivalent widths of lines in the spectra Element Element --- Lambda Wavelength 0.1nm Alpha_UMi Alpha UMi equivalent width 0.1pm HR7308(1990) HR7308(1990) equivalent width 0.1pm HR7308(1992) HR7308(1992) equivalent width 0.1pm Patricia Bauer CDS 1993 Oct 15 J_A+A_281_465.xml Model atmospheres for Vega J/A+A/281/817 J/A+A/281/817 Model atmospheres for Vega Model atmospheres for Vega F Castelli R L Kurucz Astron. Astrophys. 281 817 1994 1994A&A...281..817C stars: atmospheres stars: individual (alpha Lyr) *** No Description Available ***
The 9550K, log g = 3.95, [M/H] = -0.5 ATLAS9 model for solar He abundance The 9600K, log g = 4.00, [M/H] = -0.5 ATLAS9 model for N(He)/Ntot = 0.0634 The 9550K, log g = 3.95 ATLAS12 model for Vega abundances The 9550K, log g = 3.98 ATLAS12 model for Vega abundances The 9600K, log g = 4.00 ATLAS12 model for Vega abundances Rhox Mass depth variable=integral(0 to x)(rho(x)dx) g/cm2 T Temperature K P Gas pressure 0.1Pa Ne Electron number density cm-3 AbRoss Rosseland mass absorption coefficient cm2/g AccRad Radiative acceleration cm/s2 Vturb Microturbulence velocity cm/s Abundance change for table1a Abundance change for table2a Abundance change for table3a Abundance change for table4a Abundance change for table5a Nelem Atomic number of the element --- AC Abundance change (log(Nelem/Ntot) --- Patricia Bauer CDS 1993 Nov 12 J_A+A_281_817.xml Photometry of the Wolf-Rayet binary HD211853 in the Vilnius photometric system J/A+A/282/137 J/A+A/282/137 Vilnius Photometry of HD211853 Photometry of the Wolf-Rayet binary HD211853 in the Vilnius photometric system K Annuk Astron. Astrophys. 282 137 1994 1994A&A...282..137A binaries: general photometry stars: individual (HD 211853) stars: Wolf-Rayet *** No Description Available ***
Photometric observations of HD211853 relative to the comparison star JD Julian Date d Phase Phase: (T = JD2443690.32+6.6884*Ephem.) --- vmag v (Vilnius) magnitude mag (v-s) v-s (Vilnius) color mag (z-v) z-v (Vilnius) color mag (y-z) y-z (Vilnius) color mag (x-y) x-y (Vilnius) color mag (p-x) p-x (Vilnius) color mag (u-p) u-p (Vilnius) color mag Patricia Bauer CDS 1993 Nov 03 UNKNOWN UNKNOWN * 03-Nov-1993: first archived * 05-Jul-1995: completed JD in table2 UNKNOWN UNKNOWN Filters of the Vilnius system are: ------------------- Filter Lambda Width (A) (A) ------------------- u 3450 400 p 3740 260 x 4050 220 y 4660 260 z 5160 210 v 5440 260 s 6550 200 ------------------- J_A+A_282_137.xml Abundance gradients from disk planetary nebulae: O, Ne, S, and Ar J/A+A/282/436 J/A+A/282/436 Abundance gradients from disk planetary nebulae: Abundance gradients from disk planetary nebulae: O, Ne, S, and Ar W J Maciel J Koeppen Astron. Astrophys. 282 436 1994 1994A&A...282..436M Abundances Nebulae, planetary Galaxy: abundances Galaxy: evolution planetary nebulae: general stars: abundances *** No Description Available ***
Basic data for planetary nebulae Name Name --- PK PK designation --- Type Type --- d distance kpc r_d references to distance number=1 A78 Acker (1978) A80 Acker (1980) AGNR84 Amnuel et al. (1984) D82 Daub (1982) FV87 Freitas Pacheco and Veliz (1987) GPG86 Gathier et al. (1986a) GPP86 Gathier et al. (1986b) M84 Maciel (1984) MFO86 Maciel et al. (1986) MKH92 Mendez et al. (1992) S86 Sabbadin (1986) TPP90 Torres-Peimbert et al. (1990) --- R projected distance to the Galactic Center kpc Abundance of disk planetary nebulae Name Name --- O/H Oxygen abundances with respect to H --- r_O/H references to O/H number=2 A90 Aller (1990) AC83 Aller and Czyzak (1983) AK87 Aller and Keyes (1987) AKF88 Aller et al. (1988) B75 Boeshaar (1975) B78 Barker (1978) B83 Barker (1983) B86 Barker (1986) BLTAGB81 Beck et al. (1981) F81 French (1981) FCMC89 Freitas Pacheco et al. (1989) FM88 Fundez-Abans and Maciel (1988) FMCB91 Freitas Pacheco et al. (1991) FMC92 Freitas Pacheco et al. (1992) K70 Kaler (1970) K80 Kaler (1980) K81 Kaler (1981) K86 Kaler (1986) KAS91 Keoppen et al. (1991) KB92 Kingsburgh and Barlow (1992) KSFI91 Kaler et al. (1991) M82 Mallik (1982) MFC90 Maciel et al. (1990) NPP80 Natta et al. (1980) P84 Pottasch (1984) PDM86 Pottasch et al. (1986) PS80 Peimbert and Serrano (1980) PT83 Peimbert and Torres-Peimbert (1983) PT85 Pena and Torres-Peimbert (1985) PT87 Peimbert and Torres-Peimbert (1987) TP77 Torres-Peimbert and Peimbert (1977) TPP90 Torres-Peimbert et al. (1990) --- Ne/H Neon abundances with respect to H --- r_Ne/H references to Ne/H number=2 A90 Aller (1990) AC83 Aller and Czyzak (1983) AK87 Aller and Keyes (1987) AKF88 Aller et al. (1988) B75 Boeshaar (1975) B78 Barker (1978) B83 Barker (1983) B86 Barker (1986) BLTAGB81 Beck et al. (1981) F81 French (1981) FCMC89 Freitas Pacheco et al. (1989) FM88 Fundez-Abans and Maciel (1988) FMCB91 Freitas Pacheco et al. (1991) FMC92 Freitas Pacheco et al. (1992) K70 Kaler (1970) K80 Kaler (1980) K81 Kaler (1981) K86 Kaler (1986) KAS91 Keoppen et al. (1991) KB92 Kingsburgh and Barlow (1992) KSFI91 Kaler et al. (1991) M82 Mallik (1982) MFC90 Maciel et al. (1990) NPP80 Natta et al. (1980) P84 Pottasch (1984) PDM86 Pottasch et al. (1986) PS80 Peimbert and Serrano (1980) PT83 Peimbert and Torres-Peimbert (1983) PT85 Pena and Torres-Peimbert (1985) PT87 Peimbert and Torres-Peimbert (1987) TP77 Torres-Peimbert and Peimbert (1977) TPP90 Torres-Peimbert et al. (1990) --- S/H Sulfur abundances with respect to H --- r_S/H references to S/H number=2 A90 Aller (1990) AC83 Aller and Czyzak (1983) AK87 Aller and Keyes (1987) AKF88 Aller et al. (1988) B75 Boeshaar (1975) B78 Barker (1978) B83 Barker (1983) B86 Barker (1986) BLTAGB81 Beck et al. (1981) F81 French (1981) FCMC89 Freitas Pacheco et al. (1989) FM88 Fundez-Abans and Maciel (1988) FMCB91 Freitas Pacheco et al. (1991) FMC92 Freitas Pacheco et al. (1992) K70 Kaler (1970) K80 Kaler (1980) K81 Kaler (1981) K86 Kaler (1986) KAS91 Keoppen et al. (1991) KB92 Kingsburgh and Barlow (1992) KSFI91 Kaler et al. (1991) M82 Mallik (1982) MFC90 Maciel et al. (1990) NPP80 Natta et al. (1980) P84 Pottasch (1984) PDM86 Pottasch et al. (1986) PS80 Peimbert and Serrano (1980) PT83 Peimbert and Torres-Peimbert (1983) PT85 Pena and Torres-Peimbert (1985) PT87 Peimbert and Torres-Peimbert (1987) TP77 Torres-Peimbert and Peimbert (1977) TPP90 Torres-Peimbert et al. (1990) --- Ar/H Argon abundances with respect to H --- r_Ar/H references to Ar/H number=2 A90 Aller (1990) AC83 Aller and Czyzak (1983) AK87 Aller and Keyes (1987) AKF88 Aller et al. (1988) B75 Boeshaar (1975) B78 Barker (1978) B83 Barker (1983) B86 Barker (1986) BLTAGB81 Beck et al. (1981) F81 French (1981) FCMC89 Freitas Pacheco et al. (1989) FM88 Fundez-Abans and Maciel (1988) FMCB91 Freitas Pacheco et al. (1991) FMC92 Freitas Pacheco et al. (1992) K70 Kaler (1970) K80 Kaler (1980) K81 Kaler (1981) K86 Kaler (1986) KAS91 Keoppen et al. (1991) KB92 Kingsburgh and Barlow (1992) KSFI91 Kaler et al. (1991) M82 Mallik (1982) MFC90 Maciel et al. (1990) NPP80 Natta et al. (1980) P84 Pottasch (1984) PDM86 Pottasch et al. (1986) PS80 Peimbert and Serrano (1980) PT83 Peimbert and Torres-Peimbert (1983) PT85 Pena and Torres-Peimbert (1985) PT87 Peimbert and Torres-Peimbert (1987) TP77 Torres-Peimbert and Peimbert (1977) TPP90 Torres-Peimbert et al. (1990) --- Patricia Bauer CDS 1993 Oct 29 J_A+A_282_436.xml Duplicity in the solar neighbourhood. VII. Spectroscopic orbits of three K-dwarfs stars J/A+A/282/831 J/A+A/282/831 Duplicity in the solar neighbourhood. VII. Duplicity in the solar neighbourhood. VII. Spectroscopic orbits of three K-dwarfs stars A A Tokovinin A Duquennoy J -L Halbwachs M Mayor Astron. Astrophys. 282 831 1994 1994A&A...282..831T Binaries, spectroscopic Stars, dwarfs Stars, K-type binaries: spectroscopic stars: individual (HD 23439B, HD 237287, HD 217580) stars: late-type techniques: radial velocities *** No Description Available ***
Observations and residuals of HD 23439B Observations and residuals of HD 237287 Observations and residuals of HD 217580 HJD Heliocentric Julian Date d Vr Radial velocity km/s e_Vr Uncertaincy on radial velocity km/s O-C Velocity residual (Observed-Computed) km/s Inst Instrument CORAVEL (COR) or RVM --- Patricia Bauer CDS 1994 Mar 01 J_A+A_282_831.xml Stellar effective temperatures and angular diameters determined by the infrared flux method (IRFM): revisions using improved Kurucz LTE stellar atmospheres J/A+A/282/899 J/A+A/282/899 Stellar effective temperatures and angular Stellar effective temperatures and angular diameters determined by the infrared flux method (IRFM): revisions using improved Kurucz LTE stellar atmospheres D E Blackwell A E Lynas-Gray Astron. Astrophys. 282 899 1994 1994A&A...282..899B Effective temperatures Stars, diameters stars: atmospheres stars: fundamental parameters *** No Description Available ***
Values of Log R as a function of temperature, wavelength and surface gravity log.g Surface gravity cm/s2 Teff Effective temperature K LogR1 Ratio of integrated flux to monochromatic flux lambda 1.2467 um --- LogR2 Ratio of integrated flux to monochromatic flux lambda 2.2135 um --- LogR3 Ratio of integrated flux to monochromatic flux lambda 3.7825 um --- Effect on determined effective temperatures of using Kurucz (1992) model atmospheres instead of MARCS atmospheres Teff Effective temperature K TcJ Temperature change for use of filter J K TcK Temperature change for use of filter K K TcL Temperature change for use of filter L K Effect on determined temperatures at J, K, L for a change in surface gravity Filter Filter used --- Teff Effective temperature K Tc2 Temperature change for log g=2 K Tc3 Temperature change for log g=3 K Tc3 Temperature change for log g=4 K Effect of A(V) on effective temperatures Effect of A(V) on the integrated flux Effect of A(V) on angular diameters Teff Effective temperature K CF5 Correction factors for A(V)=0.05m --- CF10 Correction factors for A(V)=0.10m --- CF15 Correction factors for A(V)=0.15m --- CF20 Correction factors for A(V)=0.20m --- Effect of a one per cent decrease in flux at J, K, L wavelengths on temperatures Teff Effective temperature K TcJ Temperature change at J wavelength K TcK Temperature change at K wavelength K TcL Temperature change at L wavelength K Parameters of selected stars BS BS (Bright Star catalogue) number --- n_BS When *, known spectroscopic binary --- SC Spectral class --- A(V) Interstellar extinction mag V Visual magnitude mag B-V B-V color mag V-K V-K color mag log.g Surface gravity cm/s2 Fe/H Metallicity --- FT Total flux 10-9W/m2 Teff Effective temperature K D Angular diameter mas Coefficients A,B,C in the relation temperature = A+B*(V-K)+C*(V-K)**2 Type Kind of star number= Temperature = A + B(V-K) + C(V-K)^2 --- A Coefficient A number= Temperature = A + B(V-K) + C(V-K)^2 --- B Coefficient B number= Temperature = A + B(V-K) + C(V-K)^2 --- C Coefficient C number= Temperature = A + B(V-K) + C(V-K)^2 --- Comparison between determined temperatures and calculated temperatures for stars which as not been detected as spectroscopic binaries Comparison between determined temperatures and calculated temperatures for known spectroscopic binaries BS BS (Bright Star catalogue) number --- Tm Measured temperature K Tc Calculated temperature number=1 For table9, temperature = 8906 - 2625*(V-K) + 363.2*(V-K)^2 where V-K has been corrected for interstellar extinction. The stars have not been detected to be spectroscopic binaries For table10, temperature = 8825 - 2548*(V-K) + 343.9*(V-K)^2, where V-K has been corrected for interstellar extinction. The stars are known spectroscopic binaries K R Residual (measured - calculated temperature) % Comparison of IRFM effective temperatures with 'adopted' temperatures of Bell and Gustafsson BS BS (Bright Star catalogue) number --- Tbg Adopted temperature of Bell & Gustafsson number=1 Bell R.A., Gustafsson B., 1989, MNRAS, 236, 653 K Tirfm IRFM (Infrared Flux Method) effective temperature K Tirfm-Tbg Temperature differences Tirfm - Tbg % Relation between temperatures determined by Ridgway et al. and present IRFM temperatures V-K V-K color mag Tirfm IRFM effective temperature K Tr Adopted temperature of Ridgway et al. number=1 Ridgway S.T. et al., 1980, ApJ, 235, 126 K Tirfm-Tr Temperature differences Tirfm - Tr K Tirfm-Tr Temperature differences Tirfm - Tr percent % Comparison between angular diameters determined by Michelson interferometry and present IRFM determinations BS BS (Bright Star catalogue) number --- ADi IRFM angular diameter --- ADm Michelson interferometry angular diameter number=1 Mozurkewich D. et al., 1991, AJ, 101, 2207 --- ADi-ADm Angular diameter difference IRFM-Michelson % Patricia Bauer CDS 1994 Mar 14 J_A+A_282_899.xml New "flip--flop" of FK Comae Berenices J/A+A/282/L9 J/A+A/282/L9 New "flip--flop" of FK Comae Berenices New "flip--flop" of FK Comae Berenices L Jetsu I Tuominen K N Grankin S Yu Mel'nikov V S Shevchenko Astron. Astrophys. 282, L9 ??? ??? 1994 1994A&A...282L...9J Photometry Stars, variable stars: activity photometry stars: individual (FK Com) stars: variables: general *** No Description Available ***
Two new subsets of UBVR (standard Johnson) photometry of FK Com. SET Subset number --- HJD Heliocentric Julian day d U U magnitude mag B B magnitude mag V V magnitude mag R R magnitude mag F Flare detection : F=0: normal flare F=1: flare (detected with U-band) F=2: flare? (detected without U-band) --- table1.tex The tables to be processed via LaTeX Francois Ochsenbein CDS 1994 Feb 11 J_A+A_282_L9.xml Multifrequency windows on spiral galaxies. III. Internal extinction at optical and near infrared wavelengths J/A+A/283/12 J/A+A/283/12 Multifrequency windows on spiral galaxies. III. Multifrequency windows on spiral galaxies. III. Internal extinction at optical and near infrared wavelengths A Boselli G Gavazzi Astron. Astrophys. 283 12 1994 1994A&A...283...12B dust, extinction galaxies: photometry galaxies: spiral *** No Description Available ***
Target galaxies N Reference number to galaxies cluster --- Zwicky Zwicky name --- UGC UGC name --- NGC NGC name --- RA right ascension (1950) h Dec declination (1950) deg Type morphological type --- Vel recessional velocity corrected for Virgocentric infall km/s a major blue axis arcmin b minor blue axis arcmin mpg CGCG photographic magnitude mag obs H=NIR photometry, O=optical photometry --- Results of the UBV aperture photometry N Reference number to galaxies cluster --- Zwicky Zwicky name --- Diam aperture diameter arcsec V V magnitude in the individual apertures mag B B magnitude in the individual apertures mag U U magnitude in the individual apertures mag H aperture photometry N Reference number to galaxies cluster number=1 1: Cancer 2: Virgo 3: Coma/A1367 Supercluster 4: Hercules Supercluster: A2147, A2151 5: Hercules Supercluster: A2197, A2199 6: UGC --- Zwicky Zwicky name --- H(19") H mag in the 19" diaphragme mag H(27") H mag in the 27" diaphragme mag H(31.5") H mag in the 31.5" diaphragme mag H(35") H mag in the 35" diaphragme mag Patricia Bauer CDS 1993 Sep 08 J_A+A_283_12.xml Atomic Data from the Iron Project III. Rate coefficients for electron impact excitation of Boron-like ions Ne VI, Mg VIII, Al IX, Si X, S XII, Ar XIV, Ca XVI and Fe XXII. J/A+A/283/319 J/A+A/283/319 Iron Project III. B-like ions Atomic Data from the Iron Project III. Rate coefficients for electron impact excitation of Boron-like ions Ne VI, Mg VIII, Al IX, Si X, S XII, Ar XIV, Ca XVI and Fe XXII. H L Zhang M Graziani A K Pradhan Astron. Astrophys. 283 319 1994 1994A&A...283..319Z J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data *** No Description Available ***
Level indices and energies Level Level index --- LS Dominant LS state --- NeIV Ne IV energy Ry MgVIII Mg VIII energy Ry AlIX Al IX energy Ry SiX Si X energy Ry SXII S XII energy Ry ArXVI Ar XVI energy Ry CaXVI Ca XVI energy Ry FeXXII Fe XXII energy Ry Maxwellian-averaged collision strengths Elem. Element --- z Ion charge, used for the temperature --- ConfigI Initial configuration --- ConfigT Term configuration --- Gamma_e1 Maxwellian averaged collision strength for T = 100 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e2 Maxwellian averaged collision strength for T = 200 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e3 Maxwellian averaged collision strength for T = 300 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e4 Maxwellian averaged collision strength for T = 400 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e5 Maxwellian averaged collision strength for T = 500 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e6 Maxwellian averaged collision strength for T = 600 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e7 Maxwellian averaged collision strength for T = 800 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e8 Maxwellian averaged collision strength for T = 1000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e10 Maxwellian averaged collision strength for T = 1500 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e11 Maxwellian averaged collision strength for T = 2000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e12 Maxwellian averaged collision strength for T = 2500 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e13 Maxwellian averaged collision strength for T = 3000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e14 Maxwellian averaged collision strength for T = 3500 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e15 Maxwellian averaged collision strength for T = 4000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e16 Maxwellian averaged collision strength for T = 5000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e17 Maxwellian averaged collision strength for T = 6000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e18 Maxwellian averaged collision strength for T = 7000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e19 Maxwellian averaged collision strength for T = 8000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e20 Maxwellian averaged collision strength for T = 9000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e21 Maxwellian averaged collision strength for T = 10000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e22 Maxwellian averaged collision strength for T = 12000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e23 Maxwellian averaged collision strength for T = 14000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e24 Maxwellian averaged collision strength for T = 16000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e25 Maxwellian averaged collision strength for T = 18000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e26 Maxwellian averaged collision strength for T = 20000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e27 Maxwellian averaged collision strength for T = 23000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e28 Maxwellian averaged collision strength for T = 26000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e29 Maxwellian averaged collision strength for T = 30000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e30 Maxwellian averaged collision strength for T = 35000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e31 Maxwellian averaged collision strength for T = 40000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e32 Maxwellian averaged collision strength for T = 45000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Gamma_e33 Maxwellian averaged collision strength for T = 50000 x z^2 K number=1 The Maxwellian-averaged rate coefficients are tabulated for scaled electron temperatures between 100 and 50000 z^2 K, where z is the ion charge. For example, the collision strength Gamma_e1 of O IV is given for T = 100 x z^2 K (1) = 100 x 3^2 K = 900 K --- Patricia Bauer CDS 1994 Sep 01 J_A+A_283_319.xml CIV QSO absorption systems and properties of galactic haloes at high redshift J/A+A/283/759 J/A+A/283/759 CIV QSO absorption systems and properties of gal CIV QSO absorption systems and properties of galactic haloes at high redshift P Petitjean J Bergeron Astron. Astrophys. 283 759 1994 1994A&A...283..759P cosmology: observations galaxies: clusters: general galaxies: evolution galaxies: ISM quasars: absorption lines *** No Description Available ***
Absorption lines QSO QSO name --- lambda Heliocentric wavelength of absorption lines 0.1nm sigma Rest equivalent width of absorption lines 0.1nm e_sigma rms uncertainty on REW 0.1nm Iden Identification --- zabs Mean redshift --- n Component number --- logN Logarithm of the column density cm-2 e_logN rms uncertainty on logN cm-2 b Doppler parameter km/s e_b rms uncertainty on b km/s zc Redshift of the component --- Characteristic of the subcomponents QSO QSO name number= a: Savaglio et al. 1993, b: Pettini et al. 1983, c: Carswell et al. 1984, d: Wampler et al. 1993 --- Ref References --- sn Subcomponent number number= a: Savaglio et al. 1993, b: Pettini et al. 1983, c: Carswell et al. 1984, d: Wampler et al. 1993 --- z Redshift number= a: Savaglio et al. 1993, b: Pettini et al. 1983, c: Carswell et al. 1984, d: Wampler et al. 1993 --- DeltaV Relative velocity number= a: Savaglio et al. 1993, b: Pettini et al. 1983, c: Carswell et al. 1984, d: Wampler et al. 1993 km/s logN Logarithm of CIV column density number= a: Savaglio et al. 1993, b: Pettini et al. 1983, c: Carswell et al. 1984, d: Wampler et al. 1993 cm-2 b Doppler parameter for CIV number= a: Savaglio et al. 1993, b: Pettini et al. 1983, c: Carswell et al. 1984, d: Wampler et al. 1993 km/s Patricia Bauer CDS 1994 Feb 23 J_A+A_283_759.xml Integrated spectral properties of star clusters in the the near-ultraviolet J/A+A/283/805 J/A+A/283/805 Integrated spectral properties of star clusters in Integrated spectral properties of star clusters in the the near-ultraviolet E Bica D Alloin H R Schmitt Astron. Astrophys. 283 805 1994 1994A&A...283..805B galaxies: evolution galaxies: star clusters globular clusters: general Magellanic Clouds open clusters and associations: general ultraviolet: stars *** No Description Available ***
Cluster Properties Group See note 1 --- NGC NGC denomination --- Other Other name --- Age Age Myr r_Age Reference to Age number=2 Age metallicity and reddening as compiled in the BA86a except a Mould et al. 1989; b Vallenari et al. 1992; c Richtler & Nelles (1983) and Walker(1985); d Arp & Cuffey (1962) and Christian, Heasly & Janes (1985). --- Z Metallicity Sun r_Z Reference to metallicity number=2 Age metallicity and reddening as compiled in the BA86a except a Mould et al. 1989; b Vallenari et al. 1992; c Richtler & Nelles (1983) and Walker(1985); d Arp & Cuffey (1962) and Christian, Heasly & Janes (1985). --- E(B-V) Foreground reddening mag B/B+R Mironov Horizontal branch morphology parameter for the old clusters --- u_B/B+R uncertainty flag on B/B+R --- r_B/B+R Reference to B/B+R number=3 Horizontal branch morphology parameter B/B+R from Zinn(1980) except our estimates from: e Walker (1992); f Stetson (1981); g Cannon, Sagar & Hawkins (1990); h Alcaino et al. (1991); i Janes & Heasley (1991); j Bica, Barbuy & Ortolani (1993); k Alcaino (1981); l Martins, Harvel & Miller (1980); m Ortolani, Bica & Barbuy (1992); n Ortolani, Bica & Barbuy (1990); o Liller & Carney (1978); p Ortolani, Bica & Barbuy (1993). -------------------------------------------------------------------------------- Table 2 = Equivalent width in the spectral Windows ------------------------------------------------------------------------------ Window Limits (A) Main the Absorbers ------------------------------------------------------------------------------ a 3290-3332 NH; TiII; NiI b* 3332-3392 NH; TiII; TiI; CN c 3392-3420 NiI; FeI; CrII; CN d* 3420-3460 NiI; FeI; CoI; CN e 3460-3500 FeI; CN f 3500-3540 FeI; NiI g 3540-3596 FeI; CN h 3596-3626 FeI i 3626-3660 FeI; Balmer Limit; CrII; CN j 3660-3696 FeI k* 3696-3760 {HI12,13,...}; FeI M l 3760-3780 {HI11}; FeI M 1L 3780-3810 {HI10}; CN Lband 1C 3810-3822 mostly continuum in the blue clusters 2L 3822-3858 {HI9}; CN Lband; FeI; MgI; HeI 2C* 3858-3872 mostly continuum in the blue clusters 3L* 3872-3908 {HI8}; CN Lband; FeI; SiI; HeI 4 3908-3952 CaII K 5* 3952-3988 CaII H;{H_epsilon_} -------------------------------------------------------------------------------- Notes: { } indicates that the line can be in the absorption and/or emission. * indicates windows where emission lines in the e.g. HII regions and Seyfert galaxies occur ([NeV] 3346 A, [NeV] 3426 A, [OII] 3727 A, [NeIII] 3869 A and [NeIII] 3968 A). --- Equivalent Widths Groupe See note 1 --- NGC NGC number --- b Equivalent width in the [3332-3392] range 0.1nm d Equivalent width in the [3420-3460] range 0.1nm e Equivalent width in the [3460-3500] range 0.1nm f Equivalent width in the [3500-3540] range 0.1nm g Equivalent width in the [3540-3596] range 0.1nm h Equivalent width in the [3596-3626] range 0.1nm i Equivalent width in the [3626-3660] range 0.1nm k Equivalent width in the [3696-3760] range 0.1nm 1L Equivalent width in the [3780-3810] range 0.1nm 1C Equivalent width in the [3810-3822] range 0.1nm 2L Equivalent width in the [3822-3858] range 0.1nm 2C Equivalent width in the [3858-3872] range 0.1nm 3L Equivalent width in the [3872-3908] range 0.1nm 4 Equivalent width in the [3908-3952] range 0.1nm 5 Equivalent width in the [3952-3988] range 0.1nm C3540/C4020 Intensities ratio in the continuum at the wavelengths 3540/4020 --- C3660/C4020 Intensities ratio in the continuum at the wavelengths 3660/4020 --- Patricia Bauer CDS 1993 Oct 19 J_A+A_283_805.xml Elemental abundances in the old open clusters NGC 2243 and Melotte 66 J/A+A/283/911 J/A+A/283/911 Elemental abundances in the old open clusters NGC Elemental abundances in the old open clusters NGC 2243 and Melotte 66 R G Gratton G Contarini Astron. Astrophys. 283 911 1994 1994A&A...283..911G Galaxy: abundances Galaxy: evolution open clusters and associations: individual (NGC 2243, Mel 66) stars: abundances *** No Description Available ***
Equivalent widths and abundances of lines in the spectra of giants in NGC 2243 and Mel 66 Specie Specie --- Lambda Line wavelength 0.1nm EP Excitation energy eV log(gf) Oscillator strength --- n A * marks lines with detailed HFS analysis --- EW4110 Equivalent width for star 4110 in NGC2243 0.1pm n_EW4110 When s, the line was saturated --- log(A4110) Abundance for star 4110 in NGC2243 number=1 The abundances are in the scale where log n(H)=12 --- EW4209 Equivalent width for star 4209 in NGC2243 0.1pm n_EW4209 When s, the line was saturated --- log(A4209) Abundance for star 4209 in NGC2243 number=1 The abundances are in the scale where log n(H)=12 --- EW1242 Equivalent width for star 1242 in Mel 66 0.1pm n_EW1242 When s, the line was saturated --- log(A1242) Abundance for star 1242 in Mel 66 number=1 The abundances are in the scale where log n(H)=12 --- EW4151 Equivalent width for star 4151 in Mel 66 0.1pm n_EW4151 When s, the line was saturated --- log(A4154) Abundance for star 4154 in Mel 66 number=1 The abundances are in the scale where log n(H)=12 --- Patricia Bauer CDS 1993 Oct 22 J_A+A_283_911.xml HII Regions and IRAS PSC sources: the reliability of the association J/A+A/284/233 J/A+A/284/233 HII Regions and IRAS PSC sources: the reliability HII Regions and IRAS PSC sources: the reliability of the association C Codella M Felli V Natale Astron. Astrophys. 284 233 1994 1994A&A...284..233C H II regions Infrared sources Interstellar medium HII regions radio lines: ISM stars: formation *** No Description Available ***
IRAS properties of HII regions RAh Right Ascension (1950) h RAm Right Ascension (1950) min RAs Right Ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg d Distance kpc z Height from the galactic plane pc IRAS IRAS name --- l_F12 limit flag on F12 (upper limit) --- F12 IRAS flux density at 12 micron Jy l_F25 limit flag on F25 (upper limit) --- F25 IRAS flux density at 25 micron Jy l_F60 limit flag on F60 (upper limit) --- F60 IRAS flux density at 60 micron Jy l_F100 limit flag on F100 (upper limit) --- F100 IRAS flux density at 100 micron Jy l_FIR limit flag on FIR (upper limit) --- FIR Integrated infrared flux W/m2 l_LFIR limit flag on LFIR (upper limit) --- LFIR IRAS luminosity Sun R Remarks: D : double position UCHII: IRAS sources inside the WC box O : observed UCHII region (see text) --- Patricia Bauer CDS 1993 Nov 25 J_A+A_284_233.xml Long-term periodic variability in UV absorption lines of the Be star gamma Cas: on the relation with V/R variations in the Hbeta line. J/A+A/284/515 J/A+A/284/515 Long-term periodic variability in UV absorption Long-term periodic variability in UV absorption lines of the Be star gamma Cas: on the relation with V/R variations in the Hbeta line. J H Telting L Kaper Astron. Astrophys. 284 515 1994 1994A&A...284..515T Spectra, ultraviolet Stars, Be Stars, emission circumstellar matter stars: emission-line, Be stars: individual (gamma Cas) *** No Description Available ***
Results of fitting the model to residual spectra of gamma Cas Name Image number --- Vc1 N V best-fitting of the Vc Discret Absorption Component (DAC) model parameter km/s e_Vc1 rms uncertainty on Vc for N V km/s Tau_c1 N V best-fitting of the Tau_c DAC parameter --- e_Tau_c1 rms uncertainty on Tau_c for N V --- Vt1 N V best-fitting of the Vt DAC parameter km/s e_Vt1 rms uncertainty on Vt for N V km/s Ncol1 N V column density 10+12cm-2 e_Ncol1 rms uncertainty on Ncol for N V 10+12cm-2 Khi21 N V reduced Khi2 value of the best fit --- Vc2 Si IV best-fitting of the Vc DACparameter km/s e_Vc2 rms uncertainty on Vc for Si IV km/s Tau_c2 Si IV best-fitting of the Tau_c DAC parameter --- e_Tau_c2 rms uncertainty on Tau_c for Si IV --- Vt2 Si IV best-fitting of the Vt DAC parameter km/s e_Vt2 rms uncertainty on Vt for Si IV km/s Ncol2 Si IV column density 10+12cm-2 e_Ncol2 rms uncertainty on Ncol for Si IV 10+12cm-2 Khi22 Si IV reduced Khi2 value of the best fit --- Vc3 C IV best-fitting of the Vc DAC parameter km/s e_Vc3 rms uncertainty on Vc for C IV km/s Tau_c3 C IV best-fitting of the Tau_c DAC parameter --- e_Tau_c3 rms uncertainty on Tau_c for C IV --- Vt3 C IV best-fitting of the Vt DAC parameter km/s e_Vt3 rms uncertainty on Vt for C IV km/s Ncol3 C IV column density 10+12cm-2 e_Ncol3 rms uncertainty on Ncol for C IV 10+12cm-2 Khi23 C IV reduced Khi2 value of the best fit --- table4.tex LaTex version of table4 Patricia Bauer CDS 1994 Jan 18 J_A+A_284_515.xml Spectrographic study of a large sample of Kiso ultraviolet-excess galaxies. II - Discussion J/A+A/285/1 J/A+A/285/1 Spectrographic study of Kiso UV-excess galaxies Spectrographic study of a large sample of Kiso ultraviolet-excess galaxies. II - Discussion G Comte R Augarde A Chalabaev D Kunth H Maehara Astron. Astrophys. 285 1 1994 1994A&A...285....1C Galaxies, UV-excess Spectroscopy galaxies: abundances galaxies: compact galaxies: distances and redshifts galaxies: evolution galaxies: interactions galaxies: luminosity function, mass function *** No Description Available ***
Relative line ratios and oxygen abundances for 92 KUGs KUG Galaxy KUG number (in Kiso Catalog) --- [OII] log ([OII]/Hbeta) --- [OIII] log ([OIII]/Hbeta) --- [OI] log ([OI]/Hbeta) --- [NII] log ([NII]/Hbeta) --- [SII] log ([SII]/Hbeta) --- E(B-V) E(B-V) from Balmer decrement --- Te Electron temperature of the HII zone K 12+log(O/H) 12 + log([O/H]) (oxygen abundance) --- Patricia Bauer CDS 1993 Oct 19 J_A+A_285_1.xml Molecular observations of O- and C-rich circumstellar envelopes J/A+A/285/247 J/A+A/285/247 Molecular observations of O- and C-rich circum Molecular observations of O- and C-rich circumstellar envelopes V Bujarrabal A Fuente A Omont Astron. Astrophys. 285 247 1994 1994A&A...285..247B circumstellar matter radio lines: stars stars: abundances stars: AGB and post-AGB stars: late-type *** No Description Available ***
O-rich stars observational data C-rich stars observational data Other objects observational data type Type O: O-rich red-giant and supergiant C: C-rich AGB star S: S-type star PN: preplanetary nebula DE: Detached envelope number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- Name Object name number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- HCN1-0 Peak of HCN 1-0 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_HCN1-0 Remark on HCN1-0 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_HCN1-0 rms uncertainty on HCN 1-0 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aHCN1-0 Area for HCN 1-0 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_aHCN1-0 Remark on aHCN1-0 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- HNC1-0 Peak of HNC 1-0 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_HNC1-0 Remark on HNC1-0 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_HNC1-0 rms uncertainty on HNC 1-0 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aHNC1-0 Area for HNC 1-0 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_aHCN1-0 Remark on aHNC1-0 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- SiS5-4 Peak of SiS 5-4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- e_SiS5-4 rms uncertainty on SiS 5-4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aSiS5-4 Area for SiS 5-4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- HC3N10-9 Peak of HC3N 10-9 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_HC3N10-9 Remark on HC3N10-9 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_HC3N10-9 rms uncertainty on HC3N 10-9 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aHC3N10-9 Area for HC3N 10-9 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_aHC3N10-9 Remark on aHC3N10-9 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- CS3-2 Peak of CS 3-2 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_CS3-2 Remark on CS3-2 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_CS3-2 rms uncertainty on CS 3-2 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aCS3-2 Area for CS 3-2 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_aCS3-2 Remark on aCS3-2 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- CS5-4 Peak of CS 5-4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_CS5-4 Remark on CS5-4 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_CS5-4 rms uncertainty on CS 5-4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aCS5-4 Area for CS 5-4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_aCS5-4 Remark on aCS5-4 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- SiO2-1 Peak of SiO 2-1 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_SiO2-1 Remark on SiO2-1 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_SiO2-1 rms uncertainty on SiO 2-1 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aSiO2-1 Area for SiO 2-1 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_aSiO2-1 Remark on aSiO2-1 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- SiO3-2 Peak of SiO 3-2 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_SiO3-2 Remark on SiO3-2 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_SiO3-2 rms uncertainty on SiO 3-2 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aSiO3-2 Area for SiO 3-2 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_aSiO3-2 Remark on aSiO3-2 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- SO6,5-5,4 Peak of SO 6,5-5,4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_SO6,5-5,4 Remark on SO6,5-5,4 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_SO6,5-5,4 rms uncertainty on SO 6,5-5,4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- aSO6,5-5,4 Area for SO 6,5-5,4 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_aSO6,5-5,4 Remark on aSO6,5-5,4 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- 13CO2-1 Peak of 13CO 2-1 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_13CO2-1 Remark on 13CO2-1 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- e_13CO2-1 rms uncertainty on 13CO 2-1 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- a13CO2-1 Area for 13CO 2-1 number= 3mm data: 1 MHz resolution 2mm, 1mm data: 2 MHz resolution --- n_a13CO2-1 Remark on a13CO2-1 number=1 Notes are the following: * : data from other papers + : 100 kHz resolution - : 2 MHz resolution (3 mm data) : : uncertain calibration a : bad S/N ratio b : tentative detection c : neglecting the fast outflow component --- CO J=1-0 data for O-rich stars CO J=1-0 data for C-rich stars CO J=1-0 data for other objects Type Type O: O-rich red-giant and supergiant C: C-rich AGB star S: S-type star PN: preplanetary nebula DE: Detached envelope --- Name Object name --- CO1-0 Peak of CO1-0 --- n_CO1-0 + : recalibrated data * : SEST data --- cv conv. extent arcsec a_CO1-0 Area of CO1-0 --- Ref References --- Patricia Bauer CDS 1994 Jan 07 J_A+A_285_247.xml Star formation and merging in compact groups of galaxies J/A+A/285/404 J/A+A/285/404 Star formation and merging in compact groups of gal Star formation and merging in compact groups of galaxies M Moles A Del Olmo J Perea J Masegosa I Marquez V Costa Astron. Astrophys. 285 404 1994 1994A&A...285..404M galaxies: clusters: general galaxies: interactions galaxies: kinematics and dynamics galaxies: photometry *** No Description Available ***
UBV photometry of galaxies in Hickson compact groups HG Hickson group/galaxy identification --- Type Morphological type number=1 Morphological codes: 0 for ellipticals, 1 and 2 for S0 and S0a; 3 to 11 for Sa to Sm; and 12 and 13 for irregulars. --- Ap Used aperture arcsec B-V Observed (B-V) color index mag U-B Observed (U-B) color index mag B Observed B magnitude mag (B-V)c (B-V) corrected for galactic extinction and K effect mag (U-B)c (U-B) corrected for galactic extinction and K effect mag Bc B corrected for galactic extinction and K effect mag Ae Estimated effective aperture arcsec B_T Total B magnitude mag Patricia Bauer CDS 1994 Feb 22 J_A+A_285_404.xml Investigation of the semidetached eclipsing binary RZ Draconis J/A+A/285/459 J/A+A/285/459 Investigation of the semidetached eclipsing binary Investigation of the semidetached eclipsing binary RZ Draconis J M Kreiner G Pajdosz J Tremko S Zola Astron. Astrophys. 285 459 1994 1994A&A...285..459K binaries: eclipsing stars: fundamental parameters stars: individual (RZ Dra) *** No Description Available ***
Differential B photometry of RZ Dra N Number of observations --- HJD Heliocentric Julian Date - 2400000. d M_B Differential B magnitude (variable-comparison) mag Differential V photometry of RZ Dra N Number of observations --- HDJ Heliocentric Julian Date - 2400000. d M_V Differential V magnitude (variable-comparison) mag Patricia Bauer CDS 1994 Jan 27 J_A+A_285_459.xml Low-mass stars: pre-main sequence evolution and nucleosynthesis J/A+A/285/473 J/A+A/285/473 Low-mass stars: pre-main sequence evolution and Low-mass stars: pre-main sequence evolution and nucleosynthesis M Forestini Astron. Astrophys. 285 473 1994 1994A&A...285..473F nuclear reactions, nucleosynthesis, abundances stars: abundances stars: evolution stars: pre-main sequence *** No Description Available ***
Evolutionary sequences M Total mass Sun Z Star metallicity Sun n Note number=1 a: with low-temperature radiative opacity tables of Alexander (1983) b: with low- and high-temperature radiative opacity tables of Alexander (1983) and Huebner et al. (1977), respectively c: with the atmospheric temperature stratification given by the analytic T(tau) relation of Henyey et al. (1985) d: with the atmosphere integrated up to an optical depth tau = 0.001 e: with alpha = 2 f: with alpha = 1 g: with mass accretion from the beginning and during 2.5 10+6 yr, at a rate of 10-7 Msun/yr --- log(t) Star age yr L* Total luminosity Sun R Total radius Sun Teff Effective temperature K Lnuc Energetic contribution of the nuclear reaction in units of L* % Lgrav Gravitational energy release (>0) or absorption (<0) in units of L* % Mcore Mass of the radiative core Sun logTb Temperature at the base of the convective envelope K 6Li Surface 6Li abundance (relative to its initial value) --- 7Li Surface 7Li abundance (relative to its initial value) --- 9Be Surface 9Be abundance (relative to its initial value) --- table1.tex LaTex version of table1 Patricia Bauer CDS 1994 Jan 27 J_A+A_285_473.xml The galaxy population in the cluster Cl 1409+524 (3C 295) J/A+A/285/785 J/A+A/285/785 3C 295 BRri photometry The galaxy population in the cluster Cl 1409+524 (3C 295) G J Thimm H -J Roeser H Hippelein K Meisenheimer Astron. Astrophys. 285 785 1994 1994A&A...285..785T J/ApJS/78/1 : Galaxies in 7 clusters 0.35<z<0.55 (Dressler+, 1992) Clusters, galaxy Galaxies, photometry galaxies: clusters: individual (Cl 1409+524, 3C 295) galaxies: evolution stars: formation We observed the cluster Cl 1409+524 (z=0.46) with an imaging Fabry-Perot interferometer. A sequence of Fabry-Perot images (FWHM=1.0-1.3nm) was used to search for redshifted [OII]{lambda}372.7nm- and [OIII]{lambda}500.7nm line emission. We studied 144 galaxies up to a limiting continuum R-band magnitude of 22.5mag within 1 Mpc around the cluster center. Previously known emission-line galaxies in the cluster were confirmed and 17 new members with emission lines were found. Their star formation rate of 1-2M_{sun}_/yr is typical for normal spirals. We have imaged the cluster with broad band B, R and seven intermediate band filters (FWHM=10.0-20.0nm) in order to derive low-resolution spectral energy distributions of cluster galaxies. These were fitted by template spectra to estimate Hubble class and redshifts. Based on this decomposition, we derived a percentage of emission-line galaxies of 40+/-11%.
Cl 1409+524 3C 295 14 11 20.7 +52 12 09
Results from filter observations of Cl 1409+524 [TRH94] Sequential number --- y y offset according to Fig. 4 (origin: no 62) arcsec x x offset according to Fig. 4 (origin: no 62) arcsec l_Rmag Limit flag on Rmag --- Rmag R magnitude mag B-R (B-R) colour index number=1 Missing entries appear where photometry was problematic due to saturation of images, bright neighbouring objects, etc.; mag r-i (r-i) color index taken from DG 92; mag z Redshift obtained with slit spectroscopy by Dressler & Gunn (1992, Cat. <J/ApJS/78/1> --- n_z s: star --- l_z2 Limit flag on z2 number=2 In case were the {khi}^2^-minimisation gives a redshift estimate outside the investigated range (0.3<z<0.7) it is indicated by a < and > sing. --- z2 Redshift obtained from our filter observations --- n_z2 Note on z2 number=3 Entries marked with (?) indicate problems caused by very bright stars in the neighborhood of that particular object. --- e_z2 rms uncertainty on z2 --- n_e_z2 Note on e_z2 number=3 Entries marked with (?) indicate problems caused by very bright stars in the neighborhood of that particular object. --- MType Morphological type --- Rem Remarks --- James Marcout, Patricia Bauer CDS 1999 May 28 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+A_285_785.xml Spectral properties of X-ray loud extragalactic radio sources J/A+A/285/812 J/A+A/285/812 Spectral properties of X-ray loud extragalactic Spectral properties of X-ray loud extragalactic radio sources W Brinkmann J Siebert Astron. Astrophys. 285 812 1994 1994A&A...285..812B BL Lacertae objects: general galaxies: active quasars: general radio continuum: galaxies *** No Description Available ***
Spectral properties of X-ray loud extragalactic radio sources ROSAT ROSAT name (position J2000.0) --- Name Other name of the source --- Type Optical identification given in the NED --- Gamma X-ray spectral index --- e_Gamma rms uncertainty on X-ray spectral index --- N(H) Absorbing neutral hydrogen column density (best fit) 10+21cm-2 e_N(H) rms uncertainty on N(H) 10+21cm-2 chi2 Reduced chi2 for the fit (Errors are 1 sigma) --- nu Degrees of freedom for chi2 --- GammaN(H)g X-ray spectral index for fixed galactic N(H) --- e_GammaN(H)g rms uncertainty on GammaN(H)g --- N(H)g Absorbing neutral hydrogen column density for fixed galactic N(H) 10+21cm-2 chi2(g) Reduced chi2 for the fit for fixed galactic N(H) (Errors are 1 sigma) --- nu(g) Degrees of freedom for chi2(g) --- fX Unabsorbed X-ray flux in the total ROSAT energy band, computed by using the best fit values for Gamma and N(H) 10-11mW/m2 frad Radio flux at 5 GHz (Green Bank sources) or 408 MHz (Molonglo sources) Jy n_frad note number=1 c refer to the Gregory & Condon catalog m refer to the Molonglo catalog b denotes fluxes from a catalog created at MPIfR using the Green Bank data. --- ref References --- Patricia Bauer CDS 1994 Feb 23 J_A+A_285_812.xml Mode identification with the moment method in four multiperiodic beta Cephei stars: KK Velorum, nu Eri, Beta CMa, and V348 Normae J/A+A/286/136 J/A+A/286/136 Mode identification with the moment method in four Mode identification with the moment method in four multiperiodic beta Cephei stars: KK Velorum, nu Eri, Beta CMa, and V348 Normae C Aerts C Waelkens M De Pauw Astron. Astrophys. 286 136 1994 1994A&A...286..136A Stars, variable line: profiles stars: early-type stars: individual (KK Vel, nu Eri, beta, CMA, V348 Nor) stars: oscillations *** No Description Available ***
HJD and radial velocities for the measured spectra of the four stars (table12 + table13 in the paper) HJD1 Heliocentric Julian Date for KK Vel number=1 Stars Observed are: KK Vel = HD 78616 pos2000 = 09 07 42.5 -44 37 57 nu Eri = HD 29248 pos2000 = 04 36 19.1 -03 21 09 bet CMa = HD 44743 pos2000 = 06 22 41.9 -17 57 21 V348 Nor = HD 147985 pos2000 = 16 26 56.6 -43 47 57 d <v>1 Radial velocity for KK Vel km/s HJD2 Heliocentric Julian Date for nu Eri number=1 Stars Observed are: KK Vel = HD 78616 pos2000 = 09 07 42.5 -44 37 57 nu Eri = HD 29248 pos2000 = 04 36 19.1 -03 21 09 bet CMa = HD 44743 pos2000 = 06 22 41.9 -17 57 21 V348 Nor = HD 147985 pos2000 = 16 26 56.6 -43 47 57 d <v>2 Radial velocity for nu Eri km/s HJD3 Heliocentric Julian Date for beta CMa number=1 Stars Observed are: KK Vel = HD 78616 pos2000 = 09 07 42.5 -44 37 57 nu Eri = HD 29248 pos2000 = 04 36 19.1 -03 21 09 bet CMa = HD 44743 pos2000 = 06 22 41.9 -17 57 21 V348 Nor = HD 147985 pos2000 = 16 26 56.6 -43 47 57 d <v>3 Radial velocity for beta CMa km/s HJD4 Heliocentric Julian Date for V348 Nor number=1 Stars Observed are: KK Vel = HD 78616 pos2000 = 09 07 42.5 -44 37 57 nu Eri = HD 29248 pos2000 = 04 36 19.1 -03 21 09 bet CMa = HD 44743 pos2000 = 06 22 41.9 -17 57 21 V348 Nor = HD 147985 pos2000 = 16 26 56.6 -43 47 57 d <v>4 Radial velocity FOR V348 Nor km/s Patricia Bauer CDS 1994 Jan 31 J_A+A_286_136.xml 21cm observations of galaxies in the region of the Pisces-Perseus-Supercluster near the Galactic Plane J/A+A/286/17 J/A+A/286/17 21cm observations of galaxies in the region of 21cm observations of galaxies in the region of the Pisces-Perseus-Supercluster near the Galactic Plane R Seeberger W K Huchtmeier R Weinberger Astron. Astrophys. 286 17 1994 1994A&A...286...17S Galaxies, radio H I data distance scale galaxies: clusters: general galaxies: distances and redshifts radio lines: individual (21 cm) *** No Description Available ***
Observational parameters for the galaxies detected in HI Name Zone Of Avoidance Galaxy Name of the galaxy in galactic coordinate --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DiamE Optical diameter determined from Palomar red prints arcmin DiamO Optical diameter determined from Palomar blue prints arcmin I(HI) Integrated HI-flux Jy.km/s W50 Line width at 50% of the peak flux km/s W20 Line width at 20% of the peak flux km/s u_W20 uncertainty flag on W20 --- Smax Peak flux mJy e_Smax rms uncertainty on Smax mJy VHel Heliocentric radial velocity km/s n_VHel A colon indicates marginal detection --- e_VHel rms uncertainty on vHel km/s M(HI) HI-mass in 10+9 solar units Sun note See note number=1 a: These galaxies have been observed in several sessions for consistency b: Two separate profiles in one spectrum because of two galaxies within the beam at different velocities c: Unusual large profiles (either a very HI-rich galaxy or two galaxies at similar velocities) d: Several galaxies within 9 ' (beam width) are visible on the Palomar-red-prints --- L(IR) Infrared luminosity Sun u_L(IR) uncertainty flag on l_IR --- M(d) Mass of the cool dust Sun CrossId Cross-identification number=2 *: 107.12+03.41 has also been measured in the 21cm line by Martin et al. (1990). They give a radial velocity of 3504+/-5 km/s in excellent agreement with our value. --- Galaxies not detected in the HI-observations Name Zone Of Avoidance Galaxy: Name of the galaxy in galactic coordinate number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). --- RAh Right ascension 1950 number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). h RAm Right ascension 1950 number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). min RAs Right ascension 1950 number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). s DEd Declination 1950 number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). deg DEm Declination 1950 number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). arcmin DiamE Optical diameter determined from Palomar red prints number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). --- DiamO Optical diameter determined from Palomar blue prints number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). --- Type S for spiral and S? for probable spiral galaxy number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). --- rms Detections limit number= Undetected galaxies from the Uppsala Catalogue (Nilson 1973) and from the Catalogue of Galaxies Near the Galactic Plane (Weinberger 1980) are (the detection limit in mJy are given in brackets, respectively): UGC12033 (9), UGC11899 (5), UGC11874 (5), UGC11862 (6), UGC11784 (6), UGC11592 (8), WEIN4 (9). mJy Patricia Bauer CDS 1994 Feb 23 J_A+A_286_17.xml The globular cluster NGC 6652 J/A+A/286/444 J/A+A/286/444 The globular cluster NGC 6652 The globular cluster NGC 6652 S Ortolani E Bica B Barbuy Astron. Astrophys. 286 444 1994 1994A&A...286..444O Clusters, globular HR diagrams globular clusters: individual (NGC 6652) Hertzsprung-Russell (HR diagram) *** No Description Available ***
B, V photometry in NGC 6652 SN Sequence number --- X X pixel coordinate as in Fig. 1 --- Y Y pixel coordinate as in Fig. 1 --- V V magnitude mag B-V B-V colour mag V, I photometry in NGC 6652 SN Sequence number --- X X pixel coordinate as in Fig. 1 --- Y Y pixel coordinate as in Fig. 1 --- V V magnitude mag V-I V-I colour mag Patricia Bauer CDS 1993 Nov 17 J_A+A_286_444.xml Ultraviolet variations in the spectrum of the visible central star of Abell 35 J/A+A/287/591 J/A+A/287/591 Ultraviolet variations in the spectrum of the Ultraviolet variations in the spectrum of the visible central star of Abell 35 G Jasniewicz G Lapierre R Monier Astron. Astrophys. 287 591 1994 1994A&A...287..591J binaries: general planetary nebulae: individual (Abell 35) stars: chromospheres stars: close stars: variables: general *** No Description Available ***
Photometric observations of BD-22 3467 carried out in 1992 in the Geneva photometric system JD Julian day d mv Visual magnitude mag U-B U-B color mag B-V B-V color mag Patricia Bauer CDS 1994 Mar 17 J_A+A_287_591.xml HST observations of the core of globular cluster NGC 6397 J/A+A/287/769 J/A+A/287/769 UV photometry of NGC 6397 HST observations of the core of globular cluster NGC 6397 D Burgarella F Paresce G Meylan I R King P Greenfield D Baxter R Jedrzejewski A Nota R Albrecht C Barbieri J C Blades A Boksenberg P Crane J M Deharveng M J Disney P Jakobsen T M Kamperman F Macchetto C D Mackay G Weigelt Astron. Astrophys. 287 769 1994 1994A&A...287..769B Clusters, globular Photometry, ultraviolet Stars, blue binaries: close blue stragglers globular clusters: individual (NGC 6397) stars: kinematics stars: Population II ultraviolet: stars The core of the nearby and very concentrated globular cluster NGC 6397 has been imaged through the f/96-F140W, f/48-F140W, f/96-F210M and f/48-F220W ultraviolet filters of the Faint Object Camera on board the Hubble Space Telescope down to an ultraviolet limiting magnitude of ~19. The most interesting objects in the field of view are six very bright centrally concentrated, blue stragglers observed for the first time in the UV. Using these and other data from ground-based observations, we have been able to deduce from a comparison with Kurucz's atmosphere models, temperatures of ~10000K and masses of ~1.6M_{sun}_ for the four brightest ones, which is remarkably close to twice the turn-off mass of NGC 6397. This finding supports the idea that two-star mechanisms (collisions, mergers) are at the origin of the blue stragglers in the core of NGC 6397. Since the central density is very high, collisions between main sequence stars are frequent, therefore providing the best formation mechanism. We have computed the number of such collisions in the core of NGC 6397 and found it to be of the same order as the number of bright blue stragglers observed there. Thanks to the HST resolution, we have also been able to resolve one object, previously classified as a yellow straggler, into a blend of a blue straggler and three redder stars.
HST NGC 6397 17 40.9 -53 41
Positions, magnitudes and colors for the 179 objects detected in NGC 6397 Id Identification number --- Xpos X position arcsec Ypos Y position arcsec m140a f/48 camera m_140w_ magnitude mag m140-m220 f/48 camera m_140w_-m_220w_ colour mag m140b f/96 camera m_140w_ magnitude mag m140-m210 f/96 camera m_200w_-m_210w_ colour mag Vmag V magnitude mag B-V B-V color index mag Note Notes number=1 BSS: Blue stragglers star with an identification number for stars detected by Lauzeral et al. (1992A&A...262...63L) BHB: Blue horizontal branch star YSS: Yellow stragglers star --- James Marcout, Patricia Bauer CDS 1996 Nov 08 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+A_287_769.xml Luminosity variations and orbital period changes in RT Lacertae J/A+A/287/817 J/A+A/287/817 Luminosity variations and orbital period changes in Luminosity variations and orbital period changes in RT Lacertae V Keskin C Ibanoglu M C Akan S Evren Z Tunca Astron. Astrophys. 287 817 1994 1994A&A...287..817K binaries: close stars: activity stars: chromospheres stars: individual (RT Lac) stars: magnetic fields stars: variables: general *** No Description Available ***
Up-dated times of primary and secondary eclipses and residuals Min Time of minima in Julian day d E Integer eclipse cycle number --- O-C(I) Observed-calculated residual for primary minima d O-C(II) Observed-calculated residual for secondary minima d Ref References: (1) Hall & Kreiner (1980) (2) Ibanoglu et al. (1980) (3) Tunca et al. (1983) (4) Evren (1989) (5) This paper --- Patricia Bauer CDS 1994 Feb 25 J_A+A_287_817.xml Abundances of neutron-capture elements in metal-poor stars J/A+A/287/927 J/A+A/287/927 Abundances of neutron-capture elements metal-poor Abundances of neutron-capture elements in metal-poor stars R G Gratton C Sneden Astron. Astrophys. 287 927 1994 1994A&A...287..927G Galaxy: evolution nuclear reactions, nucleosynthesis, abundances stars: abundances stars: Population II Sun: abundances *** No Description Available ***
Equivalent widths and abundances for lines of n-capture elements in 19 metal-poor stars HD HD name --- E Element --- W Wavelength 0.1nm EP Potential energy eV log(gf) Oscillator strength --- l_EW Limit flag on equivalent width --- EW Equivalent width 0.1pm n When s, the line was saturated --- l_log(A) Limit flag on abundance --- log(A) Abundance --- Patricia Bauer CDS 1994 Jan 31 J_A+A_287_927.xml Meteor stream activity. 1. The annual streams. J/A+A/287/990 J/A+A/287/990 Meteor stream activity. 1. The annual streams. Meteor stream activity. 1. The annual streams. P Jenniskens Astron. Astrophys. 287 990 1994 1994A&A...287..990J comets: general meteors, meteoroids *** No Description Available ***
Catalogue of meteor streams Code code name --- Name common name of the stream --- lo solar longitude for which radiant position is valid deg RArad right ascension of radiant h DE- declination sign --- DErad declination of radiant deg dRA radiant drift in right ascension (degree of arc per degree of solar longitude) --- dDE radiant drift in declination --- Vinf geocentric entry velocity of meteoroids in the atmosphere, which includes the Earth's gravitational acceleration km/s n_Chi when *, Chi varies with solar longitude --- Chi magnitude distribution index (sporadic meteors Chi = 3.4) --- N total number of meteors observed of this stream --- Neff total number of effective observing time h Nobs number of observers that contributed to data of this stream --- Properties related to the activity curve of the meteor streams Name abbreviation name --- lo(max) solar longitude of peak position (from intersection point of slopes fitted to the data). Equinox 1950.0 number=1 ZHR = ZHRmax 10^( -B |lo - lo(max)|) deg u_lo(max) when ')', the values are for an assumed semi-major axis --- e_lo(max) rms uncertainty on lo(max) deg l_ZHRmax limit flag on ZHRmax --- ZHRmax peak rate (Zenith Hourly Rates) (1), number=2 The peak rate is in number per hour that can be seen by a standard observing in perfectly clear sky (star limiting magnitude = 6.5) and a radiant position in the zenith. h-1 u_ZHRmax when ')', the values are for an assumed semi-major axis --- e_ZHRmax rms uncertainty on ZHRmax h-1 B slope of ascending and descending branches number=1 ZHR = ZHRmax 10^( -B |lo - lo(max)|) deg-1 u_B when ')', the values are for an assumed semi-major axis --- n_B note on the slope B number=4 a: for Boo, B = 1.8 (4) b: for Gem, B = 0.39(4)/0.72(10) Values between brackets are for assumed semi-major axis --- e_B rms uncertainty on the slope B deg-1 P mean orbital period of meteoroids. number=3 The average of the mean orbital period of meteoroids is over 1/a, where a is the semi-major axis of photographically determined orbits in the literature. yr n_P : is an uncertainty flag on P * means that P is orbital period of parent comet i means infinity --- q perihelion distance AU i inclination of the orbit with respect to the ecliptic deg Pi longitude of perihelion (sum of argument of perihelion (small omega) and the ascending node(large omega)) deg M(0) mass of zero magnitude meteor g l_Rho limit flag on Rho --- Rho density of matter in the peak of the meteoroid stream 10-24g/cm3 u_Rho when ')', the values are for an assumed semi-major axis --- e_Rho rms uncertainty on the density Rho 10-24g/cm3 l_M1yr limit flag on the mass M1yr --- M1yr total mass in a flux tube of length 1 year times heliocentric velocity 10+14g u_M1yr when ')', the values are for an assumed semi-major axis --- e_M1yr rms uncertainty on the mass M1yr 10+14g l_Mtot limit flag on the mass Mtot --- Mtot total mass estimate (Mtot = M1yr x P) 10+15g n_Mtot when *, value of Mtot is for an assumed period P = 20 yr. These streams lack photographically determined orbits --- e_Mtot rms uncertainty on the mass Mtot 10+15g Results for activity profiles with a background component Name abbreviation name --- lo(max) solar longitude of peak position 1950.0 deg ZHRmax(p) peak rate for the main peak h-1 e_ZHRmax(p) rms uncertainty on ZHRmax h-1 l_Bp limit flag on the slope Bp --- Bp slope of ascending and descending branches for the main peak deg-1 n_Bp note on the slope Bp number=1 a: For Gem, Bp = (0.59/0.81) +/-0.07 Values between brackets are for assumed semi-major axis --- e_Bp rms uncertainty on the slope Bp deg-1 l_Mtot(p) limit flag on the mass Mtot(p) --- Mtot(p) total mass estimate for the main peak 10+15g e_Mtot(p) rms uncertainty on the mass Mtot(p) 10+15g ZHRmax(b) peak rate for the background h-1 e_ZHRmax(b) rms uncertainty on ZHRmax(b) h-1 Bb+ slope of ascending branch deg-1 e_Bb+ rms uncertainty on the slope Bb+ deg-1 l_Bb- limit flag on the slope Bd- --- Bb- slope of descending branch deg-1 e_Bb- rms uncertainty on the slope Bb- deg-1 Mtot(b) total mass estimate for the background 10+15g e_Mtot(b) rms uncertainty on the mass Mtot(b) 10+15g Mb/Mp background to main peak mass ratio --- e_Mb/Mp rms uncertainty on Mb/Mp --- Mtot total mass estimate 10+15g e_Mtot rms uncertainty on the mass Mtot 10+15g Patricia Bauer CDS 1994 Mar 04 J_A+A_287_990.xml The massive star content of the blue dwarf galaxy I Zw 36 from Faint Object Camera observations. J/A+A/288/413 J/A+A/288/413 Massive stars in I Zw 36 The massive star content of the blue dwarf galaxy I Zw 36 from Faint Object Camera observations. J -M Deharveng R Albrecht C Barbieri J C Blades A Boksenberg P Crane M J Disney P Jakobsen T M Kamperman I R King F Macchetto C D Mackay F Paresce G Weigelt D Baxter P Greenfield R Jedrzejewski A Nota W B Sparks Astron. Astrophys. 288 413 1994 1994A&A...288..413D Photometry Populations, stellar galaxies: individual (I Zw 36) galaxies: stellar content stars: formation stars: luminosity function, mass function ultraviolet: galaxies We have observed the blue dwarf galaxy I Zw 36 with the f/96 relay of the HST Faint Object Camera and have for the first time resolved massive stars, using the broad band filters F175W, F342W, F430W and F480LP. We have measured the fluxes of 143 of these objects and studied their characteristics in color-magnitude diagrams. A few stars may be red supergiants but their contribution to the integrated light is less than 5% in the F430W filter. The F175W-F430W color of the integrated stellar population is redder than expected from the current burst of star formation, suggesting therefore the presence of an older and unresolved underlying population. The ultraviolet measurements combined with synthetic photometry calculations allow us to place the massive stars in a bolometric magnitude vs. temperature diagram. In this diagram, the stars are compared to evolutionary tracks for different stellar masses. The current burst probably has an age less than 12Myr. We infer an Initial Mass Function, with a power-law slope in the range -1.7 to -2.6 for masses M>=20M_{sun}_. This is consistent with most of the values reported for sites of star formation in the Galaxy and the Magellanic Clouds and does not support the view of an IMF flattening at low metallicity.
HST ZW I 36 Mrk 209 12 26 16.0 +48 29 31
Photometry of stars ID Identification number --- Xpos X position number=1 1 pix = 0.002". The origin is the lower left corner of Fig.1 and X-axis is the horizontal axis. pix Ypos Y position number=1 1 pix = 0.002". The origin is the lower left corner of Fig.1 and X-axis is the horizontal axis. pix m175 Magnitude through the F175W filter mag m342 Magnitude through the F342W filter mag m430 Magnitude through the F430W filter mag James Marcout, Patricia Bauer CDS 1997 Jan 28 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+A_288_413.xml Studies of dense molecular cores in regions of massive star formation. CS J=2-1 and HCN J=1-0 observations of 11 northern cores J/A+A/288/601 J/A+A/288/601 Dense molecular cores Studies of dense molecular cores in regions of massive star formation. CS J=2-1 and HCN J=1-0 observations of 11 northern cores I Zinchenko V Forsstroem A Lapinov K Mattila Astron. Astrophys. 288 601 1994 1994A&A...288..601Z ISM: clouds ISM: molecules radio lines: ISM stars: formation *** No Description Available ***
CS mapping data for S76 CS mapping data for S153 CS mapping data for S159 CS mapping data for S184 CS mapping data for S199 CS mapping data for S255 Dalpha Gaussian line parameter Delta(alpha) arcmin Ddelta Gaussian line parameter, Delta(delta) arcmin l_TR* limit flag on TR* --- TR* Temperature scale number=1 TR* = TR/Eta_c where TR is the brightness temperature and Eta_c is the source coupling efficiency K e_TR* rms uncertainty on TR* K DeltaV Line broadening km/s e_DeltaV rms uncertainty on DeltaV km/s Vlsr LSR velocity km/s e_Vlsr rms uncertainty on Vlsr km/s Patricia Bauer CDS 1994 Mar 23 J_A+A_288_601.xml Bursting and stationary star formation in disks and nuclei of galaxies. J/A+A/288/713 J/A+A/288/713 Star formation in galaxies Bursting and stationary star formation in disks and nuclei of galaxies. C Firmani A V Tutukov Astron. Astrophys. 288 713 1994 1994A&A...288..713F VII/145 : Nearby Galaxies Catalogue (NBG) (Tully 1988) VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991) Active gal. nuclei Models, evolutionary galaxies: active galaxies: evolution galaxies: general galaxies: nuclei quasars: general Evolutionary models of disk galaxies are presented (table3), and are confronted with a sample of late type galaxies from the Tully (Nearby Galaxies, see Cat. <VII/145>) and the de Vaucouleurs (RC3, see Cat. <VII/155>) catalogues.
Sample of galaxies from Tully (1988) and RC3 Name Name of the galaxy --- MType Morphological type --- log(r) Radius of the 25th mag/arcsec+2 isophote [kpc] log(B) B luminosity [solLum] log(m_HI) HI mass [solMass] log(m_d) Dynamical mass [solMass] (B-V) Color index (B-V) mag (U-B) Color index (U-B) mag log(m_d/B) Dynamical mass to the B luminosity ratio [Sun] log(m_HI/B) HI mass to the B luminosity ratio [Sun] log(m_HI/m_d) HI mass to the dynamical mass ratio [Sun] log(sb_B) B surface brightness (solar B lum./pc2) [solMass/pc2] log(sd_HI) HI surface density (solar mass/pc2) [solMass/pc2] log(T) Total surface density (solar mass/pc2) [solMass/pc2] Correlation matrix for the sample of table1 Param Parameter designation --- log(r) Radius of the 25th mag/arcsec+2 isophote [kpc] log(m_d) Dynamical mass [solMass] log(m_HI) HI mass [solMass] log(B) B luminosity [solLum] log(T) Total surface density (solar mass/pc2) [solMass/pc2] log(sd_HI) HI surface density (solar mass/pc2) [solMass/pc2] log(sb_B) B surface brightness (solar B lum./pc2) [solLum/pc2] log(m_d/B) Dynamical mass to B luminosity ratio [Sun] log(m_HI/B) HI mass to the B luminosity ratio [Sun] log(m_HI/m_d) HI mass to the dynamical mass ratio [Sun] (B-V) Color index (B-V) mag (U-B) Color index (U-B) mag MType Morphological type --- Evolutionary models Param Parameter designation --- Age Age Gyr log(sd) Surface density (solar mass/pc2) [solMass/pc2] log(sd_g) Gas surface density (solar mass/pc2) [solMass/pc2] log(Tsb_T) Total surface brightness (solar lum/pc2) [solLum/pc2] log(sb_B) B surface brightness (solar B lum/pc2) [solLum/pc2] (B-V) Color index (B-V) mag (U-B) Color index (U-B) mag log(sfr) Star formation rate (solar mass/pc2*Gyr) [Sun/pc2/Gyr] log(T/B) Total brightness to B brightness ratio [Sun] log(sd/B) Surface density to B brightness ratio [Sun] Patricia Bauer CDS 1993 Dec 06 J_A+A_288_713.xml The Orion OB1 association. I. Stellar content J/A+A/289/101 J/A+A/289/101 Orion OB1 association. I. The Orion OB1 association. I. Stellar content A G A Brown E J De Geus P T De Zeeuw Astron. Astrophys. 289 101 1994 1994A&A...289..101B Hertzsprung-Russell (HR diagram) ISM: bubbles open clusters and associations: general open clusters and associations: individual (Orion OB1) stars: fundamental parameters stars: luminosity function, mass function *** No Description Available ***
Subgroup 1a stars derived physical parameters Subgroup 1b stars derived physical parameters Subgroup 1c stars derived physical parameters Subgroup 1d stars derived physical parameters IN Internal number of star in proposal 141 for the HIPPARCOS mission number=1 This number is also listed in: de Geus, E.J., Lub, J., van de Grift, E., 1990, A&AS 85, 915 --- HD HD or BD designation --- HIC Hipparcos Input Catalogue number --- Name Name of the star --- log(Teff) Logarithm of effective temperature K log(g) Logarithm of surface gravity cm/s2 log(L) Logarithm of luminosity Sun mv Visual magnitude mag Mv Absolute visual magnitude mag Av Visual extinction mag DM Distance modulus mag Mem. Indication of membership: blank: member PM: possible member NM: non-member --- n Note: * : the star is included in fig. 6a of paper + : the star is included in fig. 6b of paper --- MK Spectral type --- Patricia Bauer CDS 1994 Apr 08 J_A+A_289_101.xml Photoelectric light curve study of the DK Cygni system J/A+A/289/137 J/A+A/289/137 DK Cygni light curve Photoelectric light curve study of the DK Cygni system N S Awadalla Astron. Astrophys. 289 137 1994 1994A&A...289..137A binaries: eclipsing stars: individual (DK Cyg) stars: mass-loss *** No Description Available ***
UBV photoelectric light curve HJD Heliocentric Julian day d DeltaV V differential magnitude mag DeltaB B differential magnitude mag DeltaU U differential magnitude mag Patricia Bauer CDS 1994 Feb 18 J_A+A_289_137.xml The galactic abundance gradients traced by B-type stars J/A+A/289/740 J/A+A/289/740 Galactic abundance gradients The galactic abundance gradients traced by B-type stars A Kaufer T Szeifert R Krenzin B Baschek B Wolf Astron. Astrophys. 289 740 1994 1994A&A...289..740K Galaxy: abundances Galaxy: evolution stars: abundances stars: early-type *** No Description Available ***
List of the stars Name Object name --- Ref. Reference number=1 1: Hoag A.A, Applequist N.L., 1965, ApJS 12, 215 2: Hiltner W.A., 1966, IAU Symp. 24, 373 3: Hoffleit D., Jaschek C., 1982, The Bright Star Catalogue, Yale University Observatory 4: Mermilliod J.C., 1986, Catalogue of UBV Photometry and MK Spectral Types in open clusters, Institute d'Astronomie de l'Universite de Lausanne 5: Moffat A.F.J., Vogt N., 1975, A&AS 20, 85 --- V visual magnitude mag Dgal galactocentric distance kpc Measured equivalent width Ident. Laboratory wavelengths of the contributing line components --- NGC6531/2 Measured equivalent width for NGC6531/2 0.1pm NGC6823/34 Measured equivalent width for NGC6823/34 0.1pm NGC6910/2 Measured equivalent width for NGC6910/2 0.1pm NGC1893/9 Measured equivalent width for NGC1893/9 0.1pm NGC1893/10 Measured equivalent width for NGC1893/10 0.1pm Measured equivalent width Ident. Laboratory wavelengths of the contributing line components --- HR1763 Measured equivalent width for HR1763 0.1pm HR1765 Measured equivalent width for HR1765 0.1pm HR1842 Measured equivalent width for HR1842 0.1pm HR1886 Measured equivalent width for HR1886 0.1pm HR1887 Measured equivalent width for HR1887 0.1pm Measured equivalent width Ident. Laboratory wavelengths of the contributing line components number= The equivalent widths of the metallic lines and non-diffuse He I lines were measured interactively by setting the continuum individually for each line and fitting a gaussian profile. The equivalent widths of the Balmer lines were measured interactively by removing strong blend components using a spline fit over the complete profile. This profile is finally integrated in fixed wavelength intervals of typically +/-36 Angstroms (expect for S301/3 where the wavelength interval is +/-30 Angstroms). The diffuse He I lines were measured in the same way. --- hPer/717 Measured equivalent width for hPer/717 number= The equivalent widths of the metallic lines and non-diffuse He I lines were measured interactively by setting the continuum individually for each line and fitting a gaussian profile. The equivalent widths of the Balmer lines were measured interactively by removing strong blend components using a spline fit over the complete profile. This profile is finally integrated in fixed wavelength intervals of typically +/-36 Angstroms (expect for S301/3 where the wavelength interval is +/-30 Angstroms). The diffuse He I lines were measured in the same way. 0.1pm hPer/782 Measured equivalent width for hPer/782 number= The equivalent widths of the metallic lines and non-diffuse He I lines were measured interactively by setting the continuum individually for each line and fitting a gaussian profile. The equivalent widths of the Balmer lines were measured interactively by removing strong blend components using a spline fit over the complete profile. This profile is finally integrated in fixed wavelength intervals of typically +/-36 Angstroms (expect for S301/3 where the wavelength interval is +/-30 Angstroms). The diffuse He I lines were measured in the same way. 0.1pm S247/1 Measured equivalent width for S247/1 number= The equivalent widths of the metallic lines and non-diffuse He I lines were measured interactively by setting the continuum individually for each line and fitting a gaussian profile. The equivalent widths of the Balmer lines were measured interactively by removing strong blend components using a spline fit over the complete profile. This profile is finally integrated in fixed wavelength intervals of typically +/-36 Angstroms (expect for S301/3 where the wavelength interval is +/-30 Angstroms). The diffuse He I lines were measured in the same way. 0.1pm S301/3 Measured equivalent width for S301/3 number= The equivalent widths of the metallic lines and non-diffuse He I lines were measured interactively by setting the continuum individually for each line and fitting a gaussian profile. The equivalent widths of the Balmer lines were measured interactively by removing strong blend components using a spline fit over the complete profile. This profile is finally integrated in fixed wavelength intervals of typically +/-36 Angstroms (expect for S301/3 where the wavelength interval is +/-30 Angstroms). The diffuse He I lines were measured in the same way. 0.1pm S217/3 Measured equivalent width for S217/3 number= The equivalent widths of the metallic lines and non-diffuse He I lines were measured interactively by setting the continuum individually for each line and fitting a gaussian profile. The equivalent widths of the Balmer lines were measured interactively by removing strong blend components using a spline fit over the complete profile. This profile is finally integrated in fixed wavelength intervals of typically +/-36 Angstroms (expect for S301/3 where the wavelength interval is +/-30 Angstroms). The diffuse He I lines were measured in the same way. 0.1pm S208/6 Measured equivalent width for S208/6 number= The equivalent widths of the metallic lines and non-diffuse He I lines were measured interactively by setting the continuum individually for each line and fitting a gaussian profile. The equivalent widths of the Balmer lines were measured interactively by removing strong blend components using a spline fit over the complete profile. This profile is finally integrated in fixed wavelength intervals of typically +/-36 Angstroms (expect for S301/3 where the wavelength interval is +/-30 Angstroms). The diffuse He I lines were measured in the same way. 0.1pm tables.tex LaTeX version of tables 6, 7 and 8 Patricia Bauer CDS 1994 May 03 J_A+A_289_740.xml Period variations of the late type contact binaries YY Eri and AE Phe: how to use light curves outside minimum J/A+A/289/871 J/A+A/289/871 YY Eri & AE Phe Period variations of the late type contact binaries YY Eri and AE Phe: how to use light curves outside minimum C Maceroni F Van't Veer Astron. Astrophys. 289 871 1994 1994A&A...289..871M binaries: close methods: data analysis stars: individual (YY Eri, AE Phe) *** No Description Available ***
Johnson UBV observations of AE Phe Johnson BV observations of YY Eri HJD Heliocentric Julian day d U U differential magnitude (variable-comparison) mag B B differential magnitude (variable-comparison) mag V V differential magnitude (variable-comparison) mag Patricia Bauer CDS 1994 May 06 J_A+A_289_871.xml Near-IR excess of Be stars J/A+A/290/609 J/A+A/290/609 Be stars near-IR excess Near-IR excess of Be stars S M Dougherty L B F M Waters G Burki J Cote N Cramer M H Van Kerwijk A R Taylor Astron. Astrophys. 290 609 1994 1994A&A...290..609D infrared: general stars: emission-line, Be *** No Description Available ***
Excess colours of 144 Be stars HR HR number --- HD HD number --- Source Source name --- Sp Spectral type (from the Bright Star Catalogue) --- E[B-V]1 Excess [B-V] colour (calculated from spectral type) mag E[B-V]2 Excess [B-V] colour from the 2175 angstrom interstellar absorption feature (Beeckmans and Hubert-Delplace (1980)) and converted using E(B-V) = 0.84E[B-V] (Cramer, 1984) mag E[V-J] Excess [V-J] colour mag E[V-H] Excess [V-H] colour mag E[V-K] Excess [V-K] colour mag E[V-L] excess [V-L] colour mag Ref Comment for the source of the observations: a) Dougherty et al., 1991 b) Dachs et al., 1988 c) Burki et al., in preparation Visual observations from Burki et al. (in preparation) except when n_Ref. = 5 --- n_Ref If n_Ref = 5, the visual observations are taken from the catalogue of Rufener (1988) --- Patricia Bauer CDS 1994 May 30 J_A+A_290_609.xml The stellar population of the globular cluster M 3. I. Photographic photometry of 10 000 stars. J/A+A/290/69 J/A+A/290/69 M3 photographic photometry The stellar population of the globular cluster M 3. I. Photographic photometry of 10 000 stars. R Buonanno C E Corsi A Buzzoni C Cacciari F R Ferraro F Fusi Pecci Astron. Astrophys. 290 69 1994 1994A&A...290...69B globular clusters: individual (M 3) Hertzsprung-Russell (HR diagram) stars: evolution A new photographic colour-magnitude diagram for the Galactic globular cluster M 3 is presented.
Complete Bright Total sample (excluding the 96 known variables) Remaining 9491 stars Name Identification number --- m_Name Multiplicity index on Name --- Vmag V magnitude mag Bmag B magnitude mag B-V B-V colour mag X X position arcsec Y Y position arcsec Patricia Bauer CDS 1994 Nov 07 J_A+A_290_69.xml Abundances of four very metal-poor stars of the BPS survey J/A+A/290/885 J/A+A/290/885 Abundances of very metal-poor stars Abundances of four very metal-poor stars of the BPS survey F Primas P Molaro F Castelli Astron. Astrophys. 290 885 1994 1994A&A...290..885P Galaxy: abundances Galaxy: halo stars: abundances stars: Population II *** No Description Available ***
Equivalent widths and abundances for all the lines detected in our stars El. Element --- Aver A 'A' indicates average --- W Wavelength 0.1nm Chi Excitation potential eV log(gf) log of oscillation strength --- EW1 Equivalent width for CD-38 245 0.1pm n_EW1 Note on equivalent width number=1 * : Lines not included in WIDTH; + : Lines with an abundance greater than 1{sigma}. --- logA1 Abundance (logN/logN_tot_) for CD-38 245 --- e_logA1 rms uncertainty of logA1 for average --- EW2 Equivalent width for CS 22891-209 0.1pm n_EW2 Note on equivalent width number=1 * : Lines not included in WIDTH; + : Lines with an abundance greater than 1{sigma}. --- logA2 Abundance (logN/logN_tot_) for CS 22891-209 --- e_logA2 rms uncertainty of logA2 for average --- EW3 Equivalent width for CS 22897-8 0.1pm n_EW3 Note on equivalent width number=1 * : Lines not included in WIDTH; + : Lines with an abundance greater than 1{sigma}. --- logA3 Abundance (logN/logN_tot_) for CS 22897-8 --- e_logA3 rms uncertainty of logA3 for average --- EW4 Equivalent width for CS 22948-66 0.1pm n_EW4 Note on equivalent width number=1 * : Lines not included in WIDTH; + : Lines with an abundance greater than 1{sigma}. --- logA4 Abundance (logN/logN_tot_) for CS 22948-66 --- e_logA4 rms uncertainty of logA4 for average --- l_EW5 limit flag on EW5 --- EW5 Equivalent width for CS 22968-14 0.1pm n_EW5 Note on equivalent width number=1 * : Lines not included in WIDTH; + : Lines with an abundance greater than 1{sigma}. --- l_logA5 limit flag on logA5 --- logA5 Abundance (logN/logN_tot_) for CS 22968-14 --- e_logA5 rms uncertainty of logA5 for average --- logASun Solar abundance (logN/logN_tot_) Sun table3.tex LaTeX version of table3 Patricia Bauer CDS 1994 Jun 30 J_A+A_290_885.xml The active close binary system ER Vulpeculae J/A+A/291/110 J/A+A/291/110 ER Vulpeculae The active close binary system ER Vulpeculae K Olah E Budding H -I Kim P B Etzel Astron. Astrophys. 291 110 1994 1994A&A...291..110O binaries: eclipsing imaging stars: activity stars: fundamental parameters stars: individual (ER Vul) *** No Description Available ***
UBV(RI)c photometry of ER Vul JDH Heliocentric Julian day d U U magnitude mag B B magnitude mag V V magnitude mag Rc Rc magnitude mag Ic Ic magnitude mag Patricia Bauer CDS 1994 Jun 30 J_A+A_291_110.xml A Baade-Wesselink analysis of the RR Lyrae star V9 in 47 Tucanae. J/A+A/291/121 J/A+A/291/121 Study of star V9 in 47 Tuc A Baade-Wesselink analysis of the RR Lyrae star V9 in 47 Tucanae. J Storm B Nordstroem B W Carney J Andersen Astron. Astrophys. 291 121 1994 1994A&A...291..121S Photometry, infrared Radial velocities Stars, variable globular clusters: individual (47 Tuc) RR Lyrae variable stars: absolute magnitudes stars: fundamental parameters stars: horizontal-branch We present an infrared K-band light curve and a radial velocity curve for the RR Lyrae star V9 in the metal rich globular cluster 47 Tucanae ([Fe/H]=-0.71). Combining these new data with the optical photometry presented in Carney et al. (1993PASP..105..294C), we perform a Baade-Wesselink analysis and derive a distance modulus of 47 Tuc of 13.23mag+/-0.17 and absolute mean magnitudes of <M_V_>=0.32mag and <M_K_>=-0.57mag for V9. We also present a well populated visual-infrared color-magnitude diagram of the cluster, reaching from the upper red giant branch to the subgiant branch.
HV 810 47 Tuc V9 00 23.6 -72 05
K magnitudes for V9 HJD Heliocentric Julian Date at mid-exposure d Phase Phase computed according to the ephemeris HJD(max) = 2447485.385 + 0.736852 * E (days) --- Kmag Average K-band magnitude computed after binning the data according to time in bins of 11 measurements and rejecting 3 sigma outliers iteratively. mag e_Kmag rms uncertainty on Kmag mag Infrared-optical color-magnitude data for 47 Tuc ID Sequential number --- Xpos X coordinate in the IR detector frame pix Ypos Y coordinate in the IR detector frame pix K0mag Dereddened K magnitude of the star mag e_K0mag rms uncertainty on K0mag mag (V-K)0 Dereddened (V-K) color of the star mag e_(V-K)0 rms uncertainty on (V-K)0 mag Radial velocities for V9 in 47 Tuc HJD Heliocentric Julian Date at mid-exposure d Phase Phase computed according to the ephemeris HJD(max) = 2447485.385 + 0.736852 * E (days) --- RV Radial velocity km/s e_RV rms uncertainty on RV km/s Depth Depth of the CORAVEL cross-correlation dip --- e_Depth rms uncertainty on Depth --- Width Width of the CORAVEL cross-correlation dip km/s e_Width rms uncertainty on Width km/s N Average number of counts per channel for the measurement --- Patricia Bauer CDS 1996 Apr 12 Jesper Storm <jstorm@eso.org> J_A+A_291_121.xml High precision rotating neutron star models. I. Analysis of neutron star properties J/A+A/291/155 J/A+A/291/155 Rotating neutron stars models .I. High precision rotating neutron star models. I. Analysis of neutron star properties M Salgado S Bonazzola E Gourgoulhon P Haensel Astron. Astrophys. 291 155 1994 1994A&A...291..155S equation of state pulsars relativity stars: evolution stars: neutron stars: rotation *** No Description Available ***
Neutron star properties at fixed baryon mass for four equations of state (EOS). EOS EOS Equation of State used --- Hc Central pseudoenthalpy --- Ec Central energy-density 14.94x10+23kg/m/s2 Omega Rotational frequency 10+4s-1 P Period of rotation ms M Gravitational mass Sun Beta Baryon mass Sun Rcirc Circunferential (equatorial) radius km cJ/GM2 Angular momentum --- |1-lambda| Per cent error indicator --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1994 Jun 16 J_A+A_291_155.xml The occurrence of H2O masers in HII regions J/A+A/291/261 J/A+A/291/261 H2O masers in HII regions The occurrence of H2O masers in HII regions C Codella M Felli V Natale F Palagi F Palla Astron. Astrophys. 291 261 1994 1994A&A...291..261C HII regions masers radio lines: ISM stars: formation *** No Description Available ***
Summary of the observed sources RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg d Distance kpc IRAS IRAS name --- Dl Detection limit (3 r.m.s.) Jy n_Dl A 'M' indicates that maser is detected --- Rem Remarks: D : double position nd: maser known but not detected in this survey N : new detection K : kinematic distance P : photometric distance S : source associated with Sharpless regions (see the description of table1 in the paper) --- Derived parameters of the detected maser sources RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Date Observation date "DD/MM/YY" l_Fpeak limit flag --- Fpeak Flux of the strongest component Jy rms Noise of the spectrum (r.m.s.) Jy FWHM FWHM of the strongest component km/s Vpeak Velocity of the strongest component km/s Vmin Lower extreme of the emission interval km/s Vmax Upper extreme of the emission interval km/s Vres Spectral resolution km/s FH2O Integrated flux Jy.km/s LH2O Water maser luminosity Sun table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 Patricia Bauer CDS 1994 Jun 16 J_A+A_291_261.xml Dust opacities for protostellar cores J/A+A/291/943 J/A+A/291/943 Protostellar cores Dust opacities for protostellar cores V Ossenkopf T Henning Astron. Astrophys. 291 943 1994 1994A&A...291..943O dust, extinction infrared: ISM: continuum radio continuum: ISM stars: formation *** No Description Available ***
Mass absorption coefficients for the particles produced in the coagulation of an MRN distribution n(H) Gas density number=1 n(H)=0 corresponds to initial MRN size distribution of grains cm-3 Lambda0 Vacuum wavelength of light um Kappa0 Mass absorption coefficient of the whole distribution of dust grains cm2/g Lambda1 Vacuum wavelength of light with thick ice mantles um Kappa1 Mass absorption coefficient of the whole distribution of dust grains with thick ice mantles cm2/g Lambda2 Vacuum wavelength of light with thin ice mantles um Kappa2 Mass absorption coefficient of the whole distribution of dust grains with thin ice mantles cm2/g Patricia Bauer CDS 1994 Aug 31 J_A+A_291_943.xml Chemical evolution of the Magellanic Clouds. VI. Chemical composition of nine F supergiants from different regions of the Large Magellanic Cloud J/A+A/293/347 J/A+A/293/347 LMC F supergiants Chemical evolution of the Magellanic Clouds. VI. Chemical composition of nine F supergiants from different regions of the Large Magellanic Cloud V Hill S M Andrievsky M Spite Astron. Astrophys. 293 347 1995 1995A&A...293..347H galaxies: abundances Magellanic Clouds stars: abundances supergiants In an effort to increase the available information on the chemical content of the Magellanic Clouds, we investigated nine F supergiants from the field of the LMC by high-resolution spectroscopy, in order to obtain the elemental abundance ratios for C, O, {alpha}-elements, Fe peak and heavy elements. The stars are widely distributed over the LMC. An LTE analysis has given the following results: 1. All investigated stars are metal deficient ([Fe/H] value covers the interval from -0.34dex to -0.14dex; mean value: -0.27dex). 2. The iron abundance appears to be surprisingly uniform, although the stars were chosen in different regions of the LMC. The star-to star scatter is within the observation uncertainty. 3. For all stars[C/Fe]<~0 but still exceeds the value observed in LMC HII regions by +0.2dex. 4. The [O/Fe] ratio is very similar to the one found for the Galactic supergiant Canopus, and the star-to-star scatter is small ({sigma}=0.1dex) 5. Sodium does not seem to be enhanced (in average) in the LMC supergiants. 6. Among {alpha}-elements Si, S, Ca and Ti are enhanced in LMC supergiants, but Mg is slightly underabundant (with respect to Fe) when compared with solar value. 7. Heavy s- and r- process elements are overabundant by +0.3dex in average. This overabundance could be somewhat smaller for Eu, a pure r- process element.
Lines used in the analysis, with their equivalent width and individual abundance for each of the nine investigated LMC supergiants and for Canopus. Lambda Central wavelength of the line 0.1nm El. Name of the element --- El.Ion. Degree of ionization of the element (1 for neutral and 2 for ionized species) --- Xi(ex) Excitation potential of the line eV log(gf) Line transition probability in log scale --- WG244 Equivalent width of the line for star G244 0.1nm n_AG244 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG244 Abundance normalised to the Sun for G244 Sun WG258 Equivalent Width of the line for star G258 0.1nm n_AG258 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG258 Abundance normalised to the Sun for G258 Sun WG274 Equivalent Width of the line for star G274 0.1nm n_AG274 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG274 Abundance normalised to the Sun for G274 Sun WG319 Equivalent Width of the line for star G319 0.1nm n_AG319 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG319 Abundance normalised to the Sun for G319 Sun WG396 Equivalent Width of the line for star G396 0.1nm n_AG396 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG396 Abundance normalised to the Sun for G396 Sun WG406 Equivalent Width of the line for star G406 0.1nm n_AG406 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG406 Abundance normalised to the Sun for G406 Sun WG439 Equivalent Width of the line for star G439 0.1nm n_AG439 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG439 Abundance normalised to the Sun for G439 Sun WG501 Equivalent Width of the line for star G501 0.1nm n_AG501 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG501 Abundance normalised to the Sun for G501 Sun WG538 Equivalent Width of the line for star G538 0.1nm n_AG538 Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- AG538 Abundance normalised to the Sun for G538 Sun WCan Equivalent Width of the line for Canopus (taken from Luck & Lambert, 1985 and Desikachary & Hearnshaw, 1982) 0.1nm n_ACan Note on the abundance determination number=1 An asterisk following the equivalent width means that the corresponding abundance was determined by fitting the the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. "#" means that the sulfur abundance for Canopus was taken from Spite et al. (1989c) -------------------------------------------------------------------------------- Positions of the stars (Fehrenbach & Duflot, 1970, 1973) --------------------------------------------------------- Star CPD HD/HDE RA DE --------------------------------------------------------- G244 67 405 269187 05 14.08 -67 19.2 G258 269355 05 19.05 -69 48.8 G274 05 22.32 -66 57.6 G319 05 28.84 -66 03.8 G396 05 35.53 -66 47.2 G406 269868 05 36.69 -67 42.3 G439 270025 05 42.40 -68 28.8 G501 04 56.85 -67 09.7 G538 271018 05 07.11 -66 21.9 --- ACan Abundance normalised to the Sun for Canopus Sun Patricia Bauer CDS 1994 Jul 26 J_A+A_293_347.xml The outflow in the halo of M 82 J/A+A/293/703 J/A+A/293/703 Outflow in M82 halo The outflow in the halo of M 82 C D Mckeith A Greve D Downes F Prada Astron. Astrophys. 293 703 1995 1995A&A...293..703M galaxies: individual (M 82) galaxies: ISM galaxies: kinematics and dynamics galaxies: nuclei *** No Description Available ***
Position-velocity data of the minor axis outflow n_Line Line type, EL = emission line, SL = scattered line --- Line Line denomination --- d1 Distance along minor axis in arc seconds positive values: North - West, negative values: South - East arcsec d2 Distance along minor axis in linear scale, (1" equals 15pc) kpc Vel Measured velocity-systemic velocity (systemic velocity=200km/s) km/s Intensities of the blue to red velocity component Line Line denomination --- d1 Distance along minor axis in arc seconds, positive values: North - West, negative values: South - East arcsec d2 Distance along minor axis in linear scale, (1" equals 15pc) kpc IB Intensity of blue shifted component (in relative linear units) --- IR Intensity of red shifted component (in relative linear units) --- Patricia Bauer CDS 1994 Jul 26 J_A+A_293_703.xml The complex dielectric function for circumstellar silicate grains based on the IRAS data J/A+A/293/833 J/A+A/293/833 Circumstellar silicate grains The complex dielectric function for circumstellar silicate grains based on the IRAS data P David B Pegourie Astron. Astrophys. 293 833 1995 1995A&A...293..833D circumstellar matter dust, extinction infrared: stars molecular data *** No Description Available ***
Complex dielectric function Lambda Wavelength um Re Reel part of the complex dielectric function --- Im Imaginary part of the complex dielectric function -- Patricia Bauer CDS 1994 Jul 01 J_A+A_293_833.xml Atomic data from the IRON project: VI. Collision strengths and rate coefficients for Fe II, J/A+A/293/953 J/A+A/293/953 IRON project VI. FeII collision strengths Atomic data from the IRON project: VI. Collision strengths and rate coefficients for Fe II, H L Zhang A K Pradhan Astron. Astrophys. 293 953 1995 1995A&A...293..953Z J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data infrared: general plasmas ultraviolet: general Collision strengths and maxwellian averaged rate coefficients have been calculated for 10011 infrared, optical and ultraviolet transitions among 142 fine structure levels in Fe II. Collision strengths are calculated using the R-matrix method with a 38 term close-coupling target expansion and for electron energies up to 10 rydbergs. Rate coefficients are tabulated at a wide range of temperatures at which Fe II is abundant in plasma sources. A brief discussion of the calculations, sample results, and comparison with earlier works are given. The present rates for Fe II are expected to find applications in the IR, O, and UV spectral diagnostics of astrophysical objects and laboratory fusion plasmas
Configuration and observed energy (log(temp(K))=3.-5, Z = 26, N = 25, 142 fine structure levels) Level identification --- ConfigI Initial configuration (with or without one set of the intermediate spin and orbital e.g., 5D in the first level means the intermediate spin and orbital are S=2 and L=2, and none in the 6th level) --- ConfigT Term configuration --- J Total angular momentum --- E Observed energy Ry Effective collision strengths ConfigI Initial configuration --- ConfigT Term configuration --- Gamma1 Effective collision strength for T = 1000 K --- Gamma2 Effective collision strength for T = 3000 K --- Gamma3 Effective collision strength for T = 5000 K --- Gamma4 Effective collision strength for T = 7000 K --- Gamma5 Effective collision strength for T = 10000 K --- Gamma6 Effective collision strength for T = 12000 K --- Gamma7 Effective collision strength for T = 15000 K --- Gamma8 Effective collision strength for T = 17000 K --- Gamma10 Effective collision strength for T = 20000 K --- Gamma11 Effective collision strength for T = 25000 K --- Gamma12 Effective collision strength for T = 30000 K --- Gamma13 Effective collision strength for T = 35000 K --- Gamma14 Effective collision strength for T = 40000 K --- Gamma15 Effective collision strength for T = 45000 K --- Gamma16 Effective collision strength for T = 50000 K --- Gamma17 Effective collision strength for T = 60000 K --- Gamma18 Effective collision strength for T = 70000 K --- Gamma19 Effective collision strength for T = 80000 K --- Gamma20 Effective collision strength for T = 90000 K --- Gamma21 Effective collision strength for T = 100000 K --- Patricia Bauer CDS 1994 Jul 22 J_A+A_293_953.xml Atomic data from the IRON Project. VII. Radiative transition probabilities for Fe II. (Rev. November 1995) J/A+A/293/967 J/A+A/293/967 IRON Project VII. FeII radiative transitions Atomic data from the IRON Project. VII. Radiative transition probabilities for Fe II. (Rev. November 1995) S N Nahar Astron. Astrophys. 293 967 1995 1995A&A...293..967N J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data infrared: general plasmas ultraviolet: general Table ls.dat contains all LS terms considered in this work and their energy values with complete designation. Table aij.dat contains f-, S-, and A-values of transitions, both in LS multiplet and in fine structure. For the full designation of the terms in the aij.dat table check the energy table in ls.dat. A program in Fortran77, prog.f , can read the table in aji.dat and calculate lifetime in seconds from the A-values.
*LS terms Mul. Multiplet 8 = Octet, 6 = Sextet, 4 = Quartet, 2 = Doublet --- config Configuration --- SLpi Symmetry: (2S+1), L, parity of the term --- note State with * represents incomplete fs set --- D Degeneracy notation --- E(Ry,abs) Absolute energy Ry E(Ry,rel) Relative energy Ry Sultana N. Nahar Ohio Univ. ; P. Bauer, F. Ochsenbein CDS 1995 Nov 23 Sultana N. Nahar Department of Astronomy The Ohio State University 174 W. 18th Ave Columbus, OH 43210 <nahar@seaton.mps.ohio-state.edu> UNKNOWN UNKNOWN * 22-Jul-1994: the first version of the tables was provided by the author to CDS; a few modifications in the documentation and the original "prog.f" fortran program have been made with agreement of the author. * 12-Jun-1995: Revised version * 23-Nov-1995: 3 multiplets were missing J_A+A_293_967.xml Simultaneous photometric and spectroscopic monitoring of rapid variations of the Be star Eta Centauri J/A+A/294/135 J/A+A/294/135 Rapid variations of Eta Cen Simultaneous photometric and spectroscopic monitoring of rapid variations of the Be star Eta Centauri S Stefl D Baade P Harmanec L A Balona Astron. Astrophys. 294 135 1995 1995A&A...294..135S stars: activity stars: emission-line, Be stars: individual (eta Cen) *** No Description Available ***
Quantitative parameters measured in the Si III 455.26 nm line profiles of Eta Cen HJD Heliocentric Julian day d RV Stellar radial velocity km/s <v> First line moment (in the heliocentric wavelength scale) km/s <v>c First line moment (in the heliocentric wavelength scale corrected for the radial velocity RV km/s FWHM Full width at half maximum km/s LD Difference of central depth of the line with respect to the mean profile (in units of 10^-3^ x continuum) --- EW Equivalent width 0.01nm ymag Stroemgren y magnitude mag bmag Stroemgren b magnitude mag vmag Stroemgren v magnitude mag umag Stroemgren u magnitude mag c1 Stroemgren c1 colour index mag Photometric observations of Eta Cen obtained at the La Silla observatory in May-June, 1992 Photometric observations of Eta Cen obtained at the SAAO in May, 1992 HJD Heliocentric Julian day d ymag Stroemgren y magnitude mag bmag Stroemgren b magnitude mag vmag Stroemgren v magnitude mag umag Stroemgren u magnitude mag tables.tex LaTeX version of the tables Patricia Bauer CDS 1994 Aug 31 J_A+A_294_135.xml The ultraviolet absorption spectrum of the z=2.72 QSO HS 1700+6416. I. Results on heavy-element absorption systems. J/A+A/294/377 J/A+A/294/377 HS1700+6416 UV absorption The ultraviolet absorption spectrum of the z=2.72 QSO HS 1700+6416. I. Results on heavy-element absorption systems. S Vogel D Reimers Astron. Astrophys. 294 377 1995 1995A&A...294..377V cosmology: observations galaxies: abundances quasars: absorption lines quasars: individual (HS 1700+6416) *** No Description Available ***
Resonance lines and atomic parameters ion Ion Ion --- LamVac Vaccuum wavelength 0.1nm log(gf) Oscillator strength --- gamma Damping constant s-1 Absorption lines for absorber systems z Redshift --- Ion Ion --- LamVac Vacuum wavelength 0.1nm Lam(1+z) Vacuum wavelength times (1+z) 0.1nm LamObs Observed wavelength 0.1nm DLam LambdaObs-Lambda(1+z) 0.1nm FWHM Full width at half maximum 0.1nm WObs Observed equivalent width 0.1pm WFit Fitted equivalent width 0.1pm n_WFit Note on WFit, n = no line --- Com Comment --- Logarithmic column densities in metal line systems Ion Ion --- l_log(N1) limit flag on column density N1 --- log(N1) Column density at z_abs_=0.7217, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N1) Note on column density N1 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N2) limit flag on column density N2 --- log(N2) Column density at z_abs_=0.8642, b=36km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N2) Note on column density N2 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N3) limit flag on column density N3 --- log(N3) Column density at z_abs_=1.1572, b=42km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N3) Note on column density N3 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N4) limit flag on column density N4 --- log(N4) Column density at z_abs_=1.3714, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N4) Note on column density N4 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N5) limit flag on column density N5 --- log(N5) Column density at z_abs_=1.4735, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N5) Note on column density N5 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N6) limit flag on column density N6 --- log(N6) Column density at z_abs_=1.725, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N6) Note on column density N6 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N7) limit flag on column density N7 --- log(N7) Column density at z_abs_=1.8465, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N7) Note on column density N7 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N8) limit flag on column density N8 --- log(N8) Column density at z_abs_=2.1678, b=25km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N8) Note on column density N8 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N9) limit flag on column density N9 --- log(N9) Column density at z_abs_=2.189, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N9) Note on column density N9 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N10) limit flag on column density N10 --- log(N10) Column density at z_abs_=2.290, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N10) Note on column density N10 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N11) limit flag on column density N11 --- log(N11) Column density at z_abs_=2.308, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N11) Note on column density N11 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N12) limit flag on column density N12 --- log(N12) Column density at z_abs_=2.315, b=30km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N12) Note on column density N12 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N13) limit flag on column density N13 --- log(N13) Column density at z_abs_=2.433, b=38km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N13) Note on column density N13 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N14) limit flag on column density N14 --- log(N14) Column density at z_abs_=2.439, b=25km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N14) Note on column density N14 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- l_log(N15) limit flag on column density N15 --- log(N15) Column density at z_abs_=2.579, b=403km/s number=2 b is the gas velocity dispersion parameter cm-2 n_log(N15) Note on column density N15 number=1 p: peak o: outside considered range e: Echelle b: blend l: wavelength shift --- *Observed and predicted column densities z(abs) Absorption redshift --- log(N(HI))o Observed HI column density cm-2 u_log(N(HI))o Uncertainty flag on N(HI)o --- b Gas velocity dispersion parameter km/s u_b Uncertainty flag on b --- l_log(N(OIII))o Limit flag on N(OIII)o number=1 Upper limits for column densities correspond to 3 sigmas upper limits. --- log(N(OIII))o Observed OIII column density number=2 For missing ion column densities, the lines lie outside the observed spectral range or they are difficult to measure due to large unknown blends. cm-2 n_log(N(OIII))o Note on N(OIII)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- l_log(N(OIV))o Limit flag on N(OIV)o number=1 Upper limits for column densities correspond to 3 sigmas upper limits. --- log(N(OIV))o Observed OIV column density number=2 For missing ion column densities, the lines lie outside the observed spectral range or they are difficult to measure due to large unknown blends. cm-2 n_log(N(OIV))o Note on N(OIV)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- log(N(OV))o Observed OV column density number=2 For missing ion column densities, the lines lie outside the observed spectral range or they are difficult to measure due to large unknown blends. cm-2 n_log(N(OV))o Note on N(OV)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- l_log(N(OVI))o Limit flag on N(OVI)o number=1 Upper limits for column densities correspond to 3 sigmas upper limits. --- log(N(OVI))o Observed OVI column density number=2 For missing ion column densities, the lines lie outside the observed spectral range or they are difficult to measure due to large unknown blends. cm-2 n_log(N(OVI))o Note on N(OVI)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- l_log(N(NIII))o Limit flag on N(NIII)o number=1 Upper limits for column densities correspond to 3 sigmas upper limits. --- log(N(NIII))o Observed NIII column density cm-2 n_log(N(NIII))o Note on N(NIII)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- l_log(N(NIV))o Limit flag on N(NIV)o number=1 Upper limits for column densities correspond to 3 sigmas upper limits. --- log(N(NIV))o Observed NIV column density number=2 For missing ion column densities, the lines lie outside the observed spectral range or they are difficult to measure due to large unknown blends. cm-2 n_log(N(NIV))o Note on N(NIV)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- l_log(N(NV))o Limit flag on N(NV)o number=1 Upper limits for column densities correspond to 3 sigmas upper limits. --- log(N(NV))o Observed NV column density number=2 For missing ion column densities, the lines lie outside the observed spectral range or they are difficult to measure due to large unknown blends. cm-2 n_log(N(NV))o Note on N(NV)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- l_log(N(CIII))o Limit flag on N(CIII)o number=1 Upper limits for column densities correspond to 3 sigmas upper limits. --- log(N(CIII))o Observed CIII column density number=2 For missing ion column densities, the lines lie outside the observed spectral range or they are difficult to measure due to large unknown blends. cm-2 n_log(N(CIII))o Note on N(CIII)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- l_log(N(CIV))o Limit flag on N(CIV)o number=1 Upper limits for column densities correspond to 3 sigmas upper limits. --- log(N(CIV))o Observed CIV column density number=2 For missing ion column densities, the lines lie outside the observed spectral range or they are difficult to measure due to large unknown blends. cm-2 n_log(N(CIV))o Note on N(CIV)o number=3 +: Observed log(CII)=14.2 is reproduced by [C/H]=-0.52 *: Due to the poor signal-to noise of the Echelle data, these values are highly uncertain --- log(N(HII))p Predicted HII column density cm-2 log(N(OIII))p Predicted OIII column density cm-2 log(N(OIV))p Predicted OIV column density cm-2 log(N(OV))p Predicted OV column density cm-2 log(N(OVI))p Predicted OVI column density cm-2 log(N(NIII))p Predicted NIII column density cm-2 log(N(NIV))p Predicted NIV column density cm-2 log(N(NV))p Predicted NV column density cm-2 log(N(CIII))p Predicted CIII column density cm-2 log(N(CIV))p Predicted CIV column density cm-2 *Model parameters zabs Absorption redshift --- log(N(H)) Hydrogen column density cm-3 log(U) Ionization parameter (ratio of the hydrogen-ionizing photon density to the hydrogen density) --- log(T) Temperature K Dc Distance kpc log(Mc) Mass number=2 Masses were derived assuming the clouds to be spherically symmetric. solMass l_[C/H] Limit flag on [C/H] --- [C/H] Carbon abundance number=1 Solar abundances taken from Gehren (1988). --- n_[C/H] Less accurate value for [C/H] --- l_[N/H] Limit flag on [N/H] --- [N/H] Nitrogen abundance number=1 Solar abundances taken from Gehren (1988). --- n_[N/H] Less accurate value for [N/H] --- l_[O/H] Limit flag on [O/H] --- [O/H] Oxygen abundance number=1 Solar abundances taken from Gehren (1988). --- n_[O/H] Less accurate value for [O/H] --- l_[O/C] Limit flag on [O/C] --- [O/C] Oxygen to carbon abundance ratio --- n_[O/C] Less accurate value for [O/C] --- l_[N/C] Limit flag on [N/C] --- [N/C] Nitrogen to carbon abundance ratio --- *Column densities for Si, S and Ne z(abs) Absorption redshift --- l_log(N(SiII))o Limit flag on N(SiII)o --- log(N(SiII))o Observed SiII column density cm-2 n_log(N(SiII))o Note on N(SiII)o --- log(N(SiIII))o Observed SiIII column density cm-2 n_log(N(SiIII))o Note on N(SiIII)o number=1 Solar Ne abundance from Grevesse: log(Ne/H)=-3.9, Gehren: -4.2. e : Echelle data b : blend l : {lambda}-shift --- l_log(N(SiIV))o Limit flag on N(SiIV)o --- log(N(SiIV))o Observed SiIV column density cm-2 n_log(N(SiIV))o Note on N(SiIV)o number=1 Solar Ne abundance from Grevesse: log(Ne/H)=-3.9, Gehren: -4.2. e : Echelle data b : blend l : {lambda}-shift --- l_log(N(SIII))o Limit flag on N(SIII)o --- log(N(SIII))o Observed SIII column density cm-2 n_log(N(SIII))o Note on N(SIII)o number=1 Solar Ne abundance from Grevesse: log(Ne/H)=-3.9, Gehren: -4.2. e : Echelle data b : blend l : {lambda}-shift --- l_log(N(SIV))o Limit flag on N(SVI)o --- log(N(SIV))o Observed SIV column density cm-2 l_log(N(SV))o Limit flag on N(SV)o --- log(N(SV))o Observed SV column density cm-2 n_log(N(SV))o Note on N(SV)o number=1 Solar Ne abundance from Grevesse: log(Ne/H)=-3.9, Gehren: -4.2. e : Echelle data b : blend l : {lambda}-shift --- l_log(N(SVI))o Limit flag on N(SVI)o --- log(N(SVI))o Observed SVI column density cm-2 n_log(N(SVI))o Note on N(SVI)o number=1 Solar Ne abundance from Grevesse: log(Ne/H)=-3.9, Gehren: -4.2. e : Echelle data b : blend l : {lambda}-shift --- log(N(NeV))o Observed NeV column density cm-2 log(N(NeVI))o Observed NeVI column density cm-2 n_log(N(NeVI))o Note on N(NeVI)o number=1 Solar Ne abundance from Grevesse: log(Ne/H)=-3.9, Gehren: -4.2. e : Echelle data b : blend l : {lambda}-shift --- l_log(N(NeVIII))o Limit flag on N(NeVIIII)o --- log(N(NeVIII))o Observed NeVIII column density cm-2 alpha Power law index alpha ---- log(N(SiII))p Predicted SiII column density cm-2 log(N(SiIII))p Predicted SiIII column density cm-2 log(N(SiIV))p Predicted SiIV column density cm-2 log(N(SIII))p Predicted SIII column density cm-2 log(N(SIV))p Predicted SIV column density cm-2 log(N(SV))p Predicted SV column density cm-2 log(N(SVI))p Predicted SVI column density cm-2 log(N(NeV))p Predicted NeV column density cm-2 log(N(NeVI))p Predicted NeVI column density cm-2 log(N(NeVIII))p Predicted NeVIII column density cm-2 l_[Si/H] limit flag on [Si/H] --- [Si/H] Predicted Si abundance --- l_[S/H] limit flag on [S/H] --- [S/H] Predicted S abundance --- [Ne/H] Predicted Ne abundance --- u_[Ne/H] Uncertainty flag on [Ne/H] --- Interstellar absorption lines identified in HS 1700+6416 Ion Ion --- Lam Wavelength 0.1nm LamObs Observed wavelength 0.1nm DLam Difference LambdaObs - Lambda 0.1nm Wmin Detection limit number=1 For unresolved lines the instrumental FWHM divided by the strongly wavelength dependent signal-to-noise yields the observed 1sigma equivalent width limit as a function of wavelength. Values given in the table therefore correspond to 3 times the observed 1sigma equivalent width limits. 0.1nm l_log(N) Limit flag on log(N) --- log(N) Column density N of the specified ion cm-2 b Gas velocity dispersion parameter km/s EW1 HS 1700 equivalent width 0.1nm EW2 H 1821+643 equivalent width 0.1nm EW3 3C 351 equivalent width 0.1nm tables.tex LaTeX version of the tables Patricia Bauer CDS 1994 Sep 22 J_A+A_294_377.xml Variable stars in the field of the open cluster NGC 7789 J/A+A/295/101 J/A+A/295/101 Variable stars in field of NGC 7789 Variable stars in the field of the open cluster NGC 7789 K Jahn J Kaluzny S M Rucinski Astron. Astrophys. 295 101 1995 1995A&A...295..101J binaries: close binaries: eclipsing blue stragglers delta Scuti open clusters and associations: individual (NGC 7789) stars: variables: other *** No Description Available ***
NGC 7789 variable stars Name Name of the variable --- HJD Heliocentric Julian day d Vmag V magnitude mag e_Vmag rms uncertainty on V mag Patricia Bauer CDS 1994 Sep 02 J_A+A_295_101.xml Meteor stream activity. II. Meteor outbursts J/A+A/295/206 J/A+A/295/206 Meteor stream activity. II. Meteor stream activity. II. Meteor outbursts P Jenniskens Astron. Astrophys. 295 206 1995 1995A&A...295..206J meteors, meteoroids *** No Description Available ***
Catalogue of meteor outburst events that occurred between 1793 and 1993 ComType Comet type number=1 nc: near-comet type fc: far-comet type u: unknown type --- Code Name of the stream in a three letter code --- Name Common name --- Date Date of maximum activity --- RAdeg True radiant position in equinox 1950.0, corrected for zenith attraction (Earth's gravitational pull) deg DEdeg True radiant position in equinox 1950.0, corrected for zenith attraction (Earth's gravitational pull) deg u_RAdeg Uncertainty flag on radiant position --- n_RAdeg Note on radiant position --- l_Vinf Limit flag on Vinf --- Vinf Apparent entry velocity, which is the geocentric entry velocity to which is added the component due to the Earth's gravitational pull: Vinf = sqrt(V_G^2^ + 11.2^2^) km/s km/s l_Chi Limit flag on Chi --- Chi Magnitude distribution index, Chi = n(M+1)/n(M). --- Nobs1 Number of people who observed the event --- n_Nobs1 Note when Nobs1 is not detailed m: many, r: radar, s: several --- Nobs2 Number of reports that are useful for evaluating the activity profile --- E-C Time in days or years that the Earth follows (+) or leads (-) the comet at passing the node --- x_E-C Units in which E-C is expressed, d = days, y = years --- DE-C Minimum distance that the comet passes outside (+) or inside (-) the Earth's orbit --- ID Catalogue entry number --- Parameters that describe the main peak in the activity curve ComType Comet type number=1 nc: near-comet type fc: far-comet type u: unknown type --- ID Catalogue entry number -- Code Coded name --- Year Year of the event yr l_lomax limit flag on lomax --- lomax Peak position in terms of solar longitude (Eq. 1950.0) deg n_lomax When 'T' the data are in table1c --- l_ZHRmax Limit flag on ZHRmax --- ZHRmax Peak rate (meteors per hour) h-1 n_ZHRmax 'l' means 'like rain' --- e_ZHRmax rms uncertainty on ZHRmax h-1 u_ZHRmax Uncertainty flag on ZHRmax --- l_Bp Limit flag on Bp --- Bp Slope of ascending (B+) and descending (B-) branches deg-1 n_Bp A '-' indicates an interval for Bp --- Bp2 Highest value of Bp when n_Bp = '-' deg-1 e_Bp rms uncertainty on Bp deg-1 l_dE-C Limit flag on dE-C --- dE-C Difference between time of maximum activity and the node of the comet dE-C=lomax/Omega_c (or between maximum activity and point of closest approach when n_dE-C = 1 ) deg u_dE-C Uncertainty flag on dE-C --- n_dE-C When 'n_dE-C' = 1, dE-C is the difference between maximum activity and point of closest approach --- l_Pc Limit flag on Pc --- Pc Orbital period of the comet yr n_Pc When 'i', the orbital period of the comet is infinity --- q Perihelion distance number=2 For meteoroids to cross the orbit of the Earth, orbital elements are related according to: a(1-e^2) = 1 +/- e cos(w). where e = 1-q/a is the eccentricity of the orbit. AU i Inclination of orbit number=2 For meteoroids to cross the orbit of the Earth, orbital elements are related according to: a(1-e^2) = 1 +/- e cos(w). where e = 1-q/a is the eccentricity of the orbit. deg w Argument of perihelion number=2 For meteoroids to cross the orbit of the Earth, orbital elements are related according to: a(1-e^2) = 1 +/- e cos(w). where e = 1-q/a is the eccentricity of the orbit. deg M0 Mass of a zero magnitude meteor g l_rho Limit flag on 10-24rho --- rho Density of matter in the peak of the meteoroid stream. (10-24rho) 10+24g/cm3 l_Mtot Limit flag on Mtot --- Mtot Total mass in the stream. I assume cylindrical geometry. Masses are taken to be a factor less than this for near-comet type outbursts, where matter is concentrated near the comet's position. g u_Mtot Uncertainty flag on Mtot --- Parameters that describe the background component in the activity curve ComType Comet type number=1 nc: near-comet type fc: far-comet type u: unknown type --- ID Identification number --- Code Coded name --- Year Year of observation yr lomax Peak position in terms of solar longitude (Eq. 1950.0) deg u_lomax Uncertainty flag on lomax --- l_ZHRmax Limit flag on ZHRmax --- ZHRmax Peak rate (meteors per hour) h-1 e_ZHRmax rms uncertainty on ZHRmax h-1 u_ZHRmax Uncertainty flag on ZHRmax --- l_Bb+ Limit flag on Bb+ --- Bb+ Slope of ascending branches deg-1 e_Bb+ rms uncertainty on Bb+ deg-1 l_Bb- Limit flag on Bb- --- Bb- Slope of descending branches deg-1 e_Bb- rms uncertainty on Bb- deg-1 Mb Mass of the background 10+15g Mb/Mp Ratio of mass in the background component relative to the main peak --- Mtot Sum of mass estimates of background and main peak 10+15g Patricia Bauer CDS 1994 Nov 04 J_A+A_295_206.xml The central region of NGC 1365. VLA and SEST observations of the radio continuum and CO. J/A+A/295/585 J/A+A/295/585 CO observations in NGC 1365 The central region of NGC 1365. VLA and SEST observations of the radio continuum and CO. A Sandqvist S Jorsater P O Lindblad Astron. Astrophys. 295 585 1995 1995A&A...295..585S galaxies: individual (NGC 1365) galaxies: ISM galaxies: nuclei galaxies: Seyfert radio continuum: galaxies radio lines: galaxies The results of the J=1-0 and J=2-1 CO observations are presented
Result of the J=1-0 and J=2 CO observations X Offset from the nucleus along the apparent major axis --- Y Offset from the nucleus along the apparent minor axis --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec l_TA*1 Limit flag on TA*1 --- TA*1 J=1-0 peak of the antenna temperature number=1 Temperatures are ANTENNA temperatures (TA*). MAIN BEAM temperatures and integrated line intensities can be obtained by dividing by main beam efficiencies (0.66 for J=1-0; 0.54 for J=2-1). Non-detections at observed positions are indicated by "<0.02" and no entries in the other columns. When no value is given, the positions were not observed. K V1 J=1-0 peak temperature heliocentric radial velocity km/s deltaV1 J=1-0 FWHM linewidth km/s TA*dV1 Integrated line intensity of the J=1-0 line profile K.km/s l_TA*2 Limit flag on TA*2 --- TA*2 J=2-1 peak of the antenna temperature number=1 Temperatures are ANTENNA temperatures (TA*). MAIN BEAM temperatures and integrated line intensities can be obtained by dividing by main beam efficiencies (0.66 for J=1-0; 0.54 for J=2-1). Non-detections at observed positions are indicated by "<0.02" and no entries in the other columns. When no value is given, the positions were not observed. K V2 J=2-1 peak temperature heliocentric radial velocity km/s deltaV2 J=2-1 FWHM linewidth km/s TA*dV2 Integrated line intensity of the J=2-1 line profile K.km/s Patricia Bauer CDS 1994 Oct 13 J_A+A_295_585.xml Major axis kinematics of 15 early-type galaxies in the Fornax cluster. J/A+A/296/319 J/A+A/296/319 Fornax cluster early-type galaxies Major axis kinematics of 15 early-type galaxies in the Fornax cluster. M D'Onofrio S Zaggia G Longo N Caon M Capaccioli Astron. Astrophys. 296 319 1995 1995A&A...296..319D galaxies: elliptical and lenticular, cD galaxies: individual (Fornax) galaxies: kinematics and dynamics *** No Description Available ***
Major axis kinematics Name Galaxy name --- m_Name Multiplicity index on name --- r Distance from the center arcsec V(r) Rotation velocity along the major axis km/s e_V(r) rms uncertainty on velocity rotation km/s DV(r) Velocity dispersion along the major axis km/s e_DV(r) rms uncertainty velocity dispersion km/s Patricia Bauer CDS 1994 Oct 10 J_A+A_296_319.xml A search for low surface brightness dwarf galaxies in the Coma cluster core J/A+A/296/643 J/A+A/296/643 Low Surface Brightness galaxies in Coma A search for low surface brightness dwarf galaxies in the Coma cluster core I D Karachentseva V E Karachentseva G M Richter J A Vennik Astron. Astrophys. 296 643 1995 1995A&A...296..643K Clusters, galaxy Galaxies, photometry galaxies: dwarf galaxies: general galaxies: individual (Coma cluster) Using the prime focus of the 6-meter telescope, we have searched for low surface brightness dwarf galaxies in two regions in the Coma cluster: one in the center of the cluster and the other one 40arcmin to the west. The observations were carried out with a total exposure time 4x5x600sec and with a 1.2arcsec seeing. Our survey is complete down to V=25.5 and R=25.0mag. The central field shows an excess of faint galaxies (121 versus 104 in the reference field) significant at a one sigma level only. However, the central-field excess is mainly caused by the presence of faint (V=24/25mag), neutral colour (V-R=0.3/0.4) objects of low surface brightness, SB=26.0/26.5mag/arcsec^2^. These characteristics are quite consistent with those of the dwSph's in the Local Group which have typically M_v_~10mag and A~1kpc. The observed excess corresponds to a surface number density of 4gal/arcmin^2^ in the center of Coma, thus implying a total population of cluster dwarfs of ~4000 down to the limiting absolute magnitude -10mag. The number ratio of LSBD's to normal galaxies (with M<-18mag for normals) in Coma turns out to be 20:1. Such ratio is comparable to that observed in other rich clusters: A3574 (14:1) and A1367 (6:1), but is much larger than the 2:1 ratio obtained for moderate nearby clusters such as Virgo, Fornax, Antlia.
Properties of galaxies in the central Coma field Properties of galaxies in the reference field ID Galaxy identification number --- Vmag Apparent total V magnitude mag Rmag Apparent total R magnitude mag DiamV Angular diameter measured on V frame arcsec DiamR Angular diameter measured on R frame arcsec SBV Average surface brightness within DiamV mag/arcsec SBR Average surface brightness within DiamR mag/arcsec V-R Total V-R color index mag Note Notes number=1 bn: binary image df: diffuse object without a marked brightness gradient st: star-like image --- James Marcout, Patricia Bauer CDS 1997 Mar 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+A_296_643.xml A survey for medium redshift (2.2<z<3.0) optically variable QSOs. J/A+A/296/665 J/A+A/296/665 Survey of optically variables QSOs A survey for medium redshift (2.2<z<3.0) optically variable QSOs. P Veron M R S Hawkins Astron. Astrophys. 296 665 1995 1995A&A...296..665V quasars: general surveys We describe a survey for variable QSOs carried out for 15 years with the UK Schmidt telescope, using IIIaJ plates exposed behind a Schott GG395 filter. Objects brighter than B=21.0 on a reference plate and displaying a peak to peak amplitude of variability larger than B=0.35mag are selected. Plates in U, V, R and I were also obtained.
Medium redshift QSOs n_Name An '*' indicates that the QSO either is weaker than B=21.0, has a redshift z > 3.0, or does not belong to the restricted 18 sq. deg. area --- Name Name --- m_Name Multiplicity index on Name --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec z Redshift --- Bmag B magnitude mag B-V B-V colour mag U-B U-B colour mag B-R B-R colour mag dB Amplitude of variability mag M(B) Absolute B magnitude computed for Ho=50Km/s/Mpc and qo=0 in the way described by Veron-Cetty and Veron(1993) mag Notes Notes number=1 1 Cristiani et al. 1990b 2 Hawkins and Veron 1993 3 Morris et al. 1991 4 La Franca, F. 1992, private communication 5 Cristiani, S. 1992, private communication 6 AUTOFIB, AAT 1992 7 EFOSC,ESO 3.6m 1986 8 EFOSC,ESO 3.6m 1987 9 EFOSC,ESO 3.6m 1988 10 EFOSC,ESO 3.6m 1989 11 EFOSC,ESO 3.6m 1991 12 EFOSC,ESO 3.6m 1993 --- Patricia Bauer CDS 1994 Sep 20 J_A+A_296_665.xml Two reddened globular clusters projected close to the Galactic center: Palomar 6 and Djorgovski 1 J/A+A/296/680 J/A+A/296/680 Globular Clusters Djorg 1 and Pal 6 Two reddened globular clusters projected close to the Galactic center: Palomar 6 and Djorgovski 1 S Ortolani E Bica B Barbuy Astron. Astrophys. 296 680 1995 1995A&A...296..680O globular clusters: general globular clusters: individual (Pal 6, Djorg 1) Hertzsprung-Russell (HR diagram) We present NTT V,I observations of Palomar 6 and Djorgovski 1, two obscured loose clusters in crowded fields. We derive a reddening of E(B-V)=1.33+/-0.10, a distance d_{sun}_=~8.9kpc, and a metallicity of [Fe/H]=~-0.4 for Pal 6, and E(B-V)=1.71+/-0.10, d_{sun}_=~8.8kpc, and a similar metallicity ([Fe/H]=~-0.4) for Djorg 1.
Palomar 6 data Djorgovski 1 data N Stellar number --- X X coordinate pix Y Y coordinate pix Vmag V magnitude mag V-I (V-I) colour mag Patricia Bauer CDS 1994 Sep 19 J_A+A_296_680.xml H2O maser emission from semiregular variables J/A+A/296/727 J/A+A/296/727 Semiregular variables H2O maser H2O maser emission from semiregular variables M Szymczak D Engels Astron. Astrophys. 296 727 1995 1995A&A...296..727S masers stars: AGB and post-AGB stars: mass-loss surveys 107 semiregular variables of spectral type M have been observed in the H2O 6(16)-5(23) line at 22.235GHz with the 100m Effelsberg radio telescope and maser emission has been detected in 23 objects, of which 10 are new detections.
Semiregulars with H2O maser emission Name Star name --- n_Name * = new detection --- Type Star type --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Date Observation date --- Vp Peak velocity or lowest value of Vp when range of velocity (n_Vp='-') km/s n_Vp A '-' indicates a range of velocity --- Vp(high) Highest value of Vp when range of velocity km/s l_Sp limit flag on Sp --- Sp Peak flux Jy u_Sp Uncertainty flag on Sp --- l_DeltaV Limit flag on DeltaV --- DeltaV Velocity range of the maser emission km/s l_Sint Limit flag on Si --- Sint Integrated flux 10-22W/m2 Semiregulars not detected as H2O maser sources GCVS Name --- n_GCVS * = previously detected as H_2_O maser sources (Dickinson & Dinger 1982; Engels & Lewis in prep.) --- IRAS IRAS designation --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Date Observation date --- V1 Lowest velocity of velocity range km/s V2 Highest velocity of velocity range km/s F3sigma Upper limit for peak flux emission (sensitivity) Jy Asymetry of H2O maser lines Name Star name --- Date observation date --- v* Star central velocity (from Margulis et al. (1990) and Nyman et al. (1992)) km/s Sb/Si Ratio of the integrated H2O maser emission of the blue component Sb to the total integrated emission Si --- Properties of the H2O maser semiregular variables GCVS Name --- Type Variable type --- Period Period d Sp Spectral type --- [12]-[25] IRAS [12]-[25] colour --- D Distance kpc F12 Flux density at 12 {mu}m Jy.kpc2 l_log(LH2O) Limit flag on LH2O --- log(LH2O) H2O luminosity s-1 n_log(LH2O) Note on LH2O: 1 Dickinson & Dinger 1982 2 Engels & Lewis, in prep. --- Ve Expansion velocity inferred from CO data km/s dM/dt Mass loss 10-7solMass/yr tables.tex Tables 1 to 4 in LaTeX format Patricia Bauer CDS 1994 Oct 03 J_A+A_296_727.xml Stellar dynamics in E+E pairs of galaxies. I. NGC 741/742, 1587/88 and 2672/73. The data. J/A+A/297/28 J/A+A/297/28 Dynamics in E+E pairs of galaxies Stellar dynamics in E+E pairs of galaxies. I. NGC 741/742, 1587/88 and 2672/73. The data. P Bonfanti R Rampazzo F Combes P Prugniel J W Sulentic Astron. Astrophys. 297 28 1995 1995A&A...297...28B galaxies: elliptical and lenticular, cD galaxies: individual (NGC 2672, NGC 2673) galaxies: individual (NGC 741, NGC 742, NGC 1587, NGC 1588) galaxies: interactions galaxies: kinematics and dynamics We present a kinematic study of three E+E galaxy pairs, NGC 741/742, 1587/1588 (CPG 99) and 2672/2673 (CPG 175). All three pairs show a similar morphological distortion (i.e. the off-centering of inner versus outer isophotes; Davoust & Prugniel 1988) which is ascribed to the ongoing interaction. The data was obtained at the CFHT equipped with the Herzberg Spectrograph at a resolution of 0.88 Apx^-1^. NGC 741 and 2673 show significant rotation along the apparent minor axis. Both components of CPG 99 rotate very fast (with no evidence for rotation along the minor axis of either component). None of the galaxies show abnormally high central velocity dispersion. We report some of the first clear detections of well defined velocity dispersion curves for interacting pairs. They show a systematic decrease with distance from the center, as expected for normal ellipticals. They do not show obvious heating in the outer parts as was previously reported. NGC 741 and 2672 show, respectively, possible U and inverse U-shaped structure in their velocity profiles.
Kinematic data NGC NGC name --- P.A. Position angle deg Radius Radius arcsec V(r) Velocity as function of radius km/s e_V(r) rms uncertainty on V(r) km/s sigma_V(r) Velocity dispersion as function of radius km/s e_sigma_V(r) rms uncertainty on sigma_V km/s Patricia Bauer CDS 1994 Oct 20 J_A+A_297_28.xml Photometric elements, absolute dimensions and evolutionary status of the eclipsing binary HU Tauri (HR 1471) J/A+A/297/359 J/A+A/297/359 Eclipsing binary HU Tauri Photometric elements, absolute dimensions and evolutionary status of the eclipsing binary HU Tauri (HR 1471) M Parthasarathy M B K Sarma P Vivekananda Rao Astron. Astrophys. 297 359 1995 1995A&A...297..359P binaries: close binaries: spectroscopic stars: evolution stars: fundamental parameters stars: individual (HU Tau, HR 1471) The photometric elements of HU Tauri are derived from an analysis of its blue and visual light curves using the Wilson and Devinney (1971, ApJ 166, 605) light curve synthesis method. Combining the photometric elements and spectroscopic orbital elements the absolute dimensions of the system are derived.
HU Tauri blue and yellow light curves Phase phase d DBmag Differential B magnitude (HU Tau-HR 1472) mag DVmag Differential V magnitude (HU Tau-HR 1472) mag Nobs Number of observations forming the normal points --- Patricia Bauer CDS 1994 Oct 17 J_A+A_297_359.xml A survey of main-line OH maser emission from semiregular variables J/A+A/297/494 J/A+A/297/494 OH maser from semiregular variables A survey of main-line OH maser emission from semiregular variables M Szynczak A M Le Squeren P Sivagnanam F Tran Minh A Fournier Astron. Astrophys. 297 494 1995 1995A&A...297..494S circumstellar matter masers radio lines: stars stars: AGB and post-AGB stars: mass-loss We have made a high sensivity (~0.15Jy) search in the OH main-lines for maser emission from a sample of 181 semiregular variables.
Semiregulars with OH maser emission IRAS IRAS name --- GCVS GCVS name --- Type Type of variability --- Date Observation date "DD/MM/YY" l_Sp1(1665) limit flag on Sp1(1665) --- Sp1(1665) First peak flux density at 1665MHz Jy Vp1(1665) Radial velocity of Sp1(1665) number=1 V is the radial velocity relative to the local standard of rest Vlsr km/s Sp2(1665) Second peak flux density at 1665MHz Jy Vp2(1665) Radial velocity of Sp2(1665) number=1 V is the radial velocity relative to the local standard of rest Vlsr km/s Sp3(1665) Third peak flux density at 1665MHz Jy Vp3(1665) Radial velocity of Sp3(1665) number=1 V is the radial velocity relative to the local standard of rest Vlsr km/s Sp4(1665) 4th peak flux density at 1665MHz Jy V4(1665) Radial velocity of Sp4(1665) number=1 V is the radial velocity relative to the local standard of rest Vlsr km/s Sint(1665) Integrated flux of the entire OH profile at 1665MHz Jy.km/s l_Sp1(1667) limit flag on Sp1(1667) --- Sp1(1667) First peak flux density at 1667MHz Jy Vp1(1667) Radial velocity of Sp1(1667) number=1 V is the radial velocity relative to the local standard of rest Vlsr km/s Sp2(1667) Second peak flux density at 1667MHz Jy Vp2(1667) Radial velocity of Sp2(1667) number=1 V is the radial velocity relative to the local standard of rest Vlsr km/s Sint(1667) Integrated flux of the entire OH profile at 1667MHz Jy.km/s Notes Notes number=2 a new detection b Le Squeren et al. (1992) c Dickinson et al. (1986) d Nguyen-Q-Rieu et al. (1971) e tentative detection --- Upper limits for undetected semiregular IRAS IRAS name --- GCVS GCVS name --- Type Type of variability --- Date Observing date (month, year) --- V1 Lowest velocity of the velocity range km/s V2 Highest velocity of the velocity range km/s n_V1 L = LSR, H = heliocentric --- S 1 sigma upper limit flux density number=1 1 sigma = 50 mJy for SRb stars in a mean values for this group. mJy Ref References number=2 References: 1 Caswell et al.(1971) 2 Paschenko et al.(1971) 3 Fillit et al. (1972) 4 Wilson & Barrett (1972) 5 Wilson & Riegel (1973) 6 Kolena & Pataki (1977) 7 Fix & Weisberg (1978) 8 Paschenko & Rudnitskij (1979) 9 Bowers (1981) 10 Fix & Claussen (1984) 11 Ukita & Le Squeren (1984) 12 Dickinson et al. (1986) 13 Eder et al. (1988) --- Patricia Bauer CDS 1994 Oct 20 J_A+A_297_494.xml The spatial distribution of supernovae in paired and interacting galaxies J/A+A/297/49 J/A+A/297/49 Supernovae spatial distribution The spatial distribution of supernovae in paired and interacting galaxies A R Petrosian M Turatto Astron. Astrophys. 297 49 1995 1995A&A...297...49P galaxies: interactions galaxies: starburst supernovae: general In order to investigate the location of supernovae (SNe) in paired and interacting galaxies, the 54 supernovae discovered up to May 1993 in 14 Isolated Pairs of Galaxies and in 32 Interacting Systems were taken as a sample and studied.
Interacting galaxies with supernovae Isolated Pairs of galaxies with Supernovae Gal Galaxy name --- MType Galaxy type --- log(Lp/Ln) Logarithmic ratio of the blue luminosity of the SN parent galaxy to that of its close neighbour, corrected for galactic absorption --- alpha Far Infrared spectral index number=1 Computed via relation: {alpha}^100^_60_=log(S_{nu}_(100)/S_{nu}_(60)) /log(60/100), where S_{nu}_(100) and S_{nu}_(60) are the FIR flux densities at the wavelengths 60um and 100um, respectively. --- log(LFIR/Lb) Far infrared to B luminosity ratio --- D(V) Difference of the velocities of the parent and the neighbour galaxy, retrieved from the most recent literature km/s SN Supernova name --- SNType Supernova type --- theta Distance of the SN from the center of the galaxy in units of the galactic radius at 25 mag/arcsec^2^ --- theta0 Corrected value of theta for the tilting of the parent galaxies along the line of sight --- r/R1,2 Ratio of the projected distance of the SN from the parent galaxy nuclei to the projected separation between components of the paired/interacting galaxies --- PA Position angle of the SNE with respect to the neighbours number=2 The PA is computed clockwise with the companion placed at 180deg. deg Patricia Bauer CDS 1994 Nov 07 J_A+A_297_49.xml Analysis of the moderately Li-rich giant HD 146850 J/A+A/297/503 J/A+A/297/503 HD 146850 Analysis of the moderately Li-rich giant HD 146850 B V Castilho B Barbuy J Gregorio-Hetem Astron. Astrophys. 297 503 1995 1995A&A...297..503C stars: abundances stars: individual (HD 146850) We report the identification of 3 Li-rich giants discovered in an ongoing survey based on IRAS colours. A detailed analysis of one of these, HD 146850, is presented here. High resolution spectra were obtained for this star, using CASPEC at the 3.6m telescope of ESO.
Data Lam Wavelength 0.1nm Element Element --- Ion Ionisation stage --- Exc Excitation potential eV log(gf) Oscillator strength --- W Equivalent width 0.1pm Patricia Bauer CDS 1994 Sep 20 J_A+A_297_503.xml Extragalactic large-scale structures behind the southern Milky Way. I. Redshifts obtained at the SAAO in the Hydra/Antlia extension. J/A+A/297/617 J/A+A/297/617 Hydra/Antlia extension redshifts Extragalactic large-scale structures behind the southern Milky Way. I. Redshifts obtained at the SAAO in the Hydra/Antlia extension. R C Kraan-Korteweg A P Fairall C Balkowski Astron. Astrophys. 297 617 1995 1995A&A...297..617K galaxies: clusters: general galaxies: distances and redshifts large-scale structure of universe Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg<~l<~296deg, |b|<~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.
Galaxy with absorption and emission features heliocentric velocity Id Running number of identified galaxy as in "A Catalogue of 3279 Galaxies in the Zona of Avoidance in the Hydra/Antlia Extension (Kraan-Korteweg, 1994) --- Name Identification in Lauberts Catalogue (1982) --- RAh Right ascension B1950 h RAm Right ascension B1950 min RAs Right ascension B1950 s DE- Declination sign --- DEd Declination B1950 deg DEm Declination B1950 arcmin DEs Declination B1950 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg a Major axis arcsec b Minor axis arcsec Bmag B magnitude estimated from the IIIaJ ESO/SRC film copy mag MType Morphological type --- HVa Heliocentric velocity from absorption line features km/s e_HVa rms uncertainty on absorption velocity km/s HVe Heliocentric velocity from emission line features km/s e_HVe rms uncertainty on emission velocity km/s EL1 Code for identified emission line number=1 Codes for identified emission line: 1: [OII] 3727A 2: H{gamma} 4340A 3: H{beta} 4861A 4: [OIII] 4959A 5: [OIII] 5007A 6: H{alpha} 6563A 7: [NII] 6584A --- EL2 Code for identified emission line number=1 Codes for identified emission line: 1: [OII] 3727A 2: H{gamma} 4340A 3: H{beta} 4861A 4: [OIII] 4959A 5: [OIII] 5007A 6: H{alpha} 6563A 7: [NII] 6584A --- EL3 Code for identified emission line number=1 Codes for identified emission line: 1: [OII] 3727A 2: H{gamma} 4340A 3: H{beta} 4861A 4: [OIII] 4959A 5: [OIII] 5007A 6: H{alpha} 6563A 7: [NII] 6584A --- EL4 Code for identified emission line number=1 Codes for identified emission line: 1: [OII] 3727A 2: H{gamma} 4340A 3: H{beta} 4861A 4: [OIII] 4959A 5: [OIII] 5007A 6: H{alpha} 6563A 7: [NII] 6584A --- EL5 Code for identified emission line number=1 Codes for identified emission line: 1: [OII] 3727A 2: H{gamma} 4340A 3: H{beta} 4861A 4: [OIII] 4959A 5: [OIII] 5007A 6: H{alpha} 6563A 7: [NII] 6584A --- EL6 Code for identified emission line number=1 Codes for identified emission line: 1: [OII] 3727A 2: H{gamma} 4340A 3: H{beta} 4861A 4: [OIII] 4959A 5: [OIII] 5007A 6: H{alpha} 6563A 7: [NII] 6584A --- Rem Code for remarks to table 1 number=2 Codes for additional remarks: 1: The spectrum of KK527 shows this to be a Seyfert 1 galaxy. 2: The spectrum of KK1963=L92-10 was measured at different sites and - based on the emission lines [OII], H(beta),[OIII], H(alpha), [NII] - the following velocities were obtained: V(hel)=134, 26, 87, 10, 35, 6, 100 +/- 58 km/s. The velocity given in Table1 is the mean of all these velocities. Further details are given below. 3: Due to superposition of a star on the galaxy KK2508=L62-10 the exposures were centred slightly west of the centre of the object. For some of the galaxies other redshift measurements are available as well (cf. section 2.2.2): A: V(hel)= 2916+/-45km/s by Strauss et al. 1992, for KK1517=L126-24. B: V(hel) = 1830km/s by Acker et al. 1991 for KK1853 (cf. special cases). C: V(hel)= 5523km/s by Dressler 1991 for KK2992=L170-3. --- Galaxy without detected heliocentric velocity Id Running number of identified galaxy as in "A Catalogue of 3279 Galaxies in the Zona of Avoidance in the Hydra/Antlia Extension (Kraan-Korteweg, 1994) --- Name Identification in Lauberts Catalogue (1982) --- RAh Right ascension B1950 h RAm Right ascension B1950 min RAs Right ascension B1950 s DE- Declination sign --- DEd Declination B1950 deg DEm Declination B1950 arcmin DEs Declination B1950 arcsec u_DEm Uncertainty flag on declination --- GLON Galactic longitude deg GLAT Galactic latitude deg a Major axis arcsec b Minor axis arcsec Bmag B magnitude estimated from the IIIaJ ESO/SRC film copy mag MType Morphological type --- Rem Remark describing reason for non-detection of velocity --- Galaxy with detected heliocentric velocity Id Running number of identified galaxy as in "A Catalogue of 3279 Galaxies in the Zone of Avoidance in the Hydra/Antlia Extension (Kraan-Korteweg, 1994) --- Name Identification in Lauberts Catalogue (1982) --- RAh Right ascension B1950 h RAm Right ascension B1950 min RAs Right ascension B1950 s DE- Declination sign --- DEd Declination B1950 deg DEm Declination B1950 arcmin DEs Declination B1950 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg a Major axis arcsec b Minor axis arcsec Bmag B magnitude estimated from the IIIaJ ESO/SRC film copy mag MType Morphological type --- HV Heliocentric velocity km/s e_HV rms uncertainty on HV km/s n_HV Code for source of the velocity number=1 Codes for sources: 1: The Southern Redshift Catalogue and Plots by Fairall and Jones (1991) 2: The General Catalog of HI-Observations of Galaxies by Huchtmeier and Richter (1989) 3: The 2Jy IRAS Redshift Survey by Strauss et al. (1992) --- Patricia Bauer CDS 1994 Nov 28 J_A+A_297_617.xml A ROSAT X-ray study of the Praesepe cluster J/A+A/298/115 J/A+A/298/115 ROSAT study of Praesepe A ROSAT X-ray study of the Praesepe cluster S Randich J H M M Schmitt Astron. Astrophys. 298 115 1995 1995A&A...298..115R open clusters and associations: individual (Praesepe) stars: coronae X-rays: stars We present the results of the ROSAT PSC observations of the Praesepe cluster. 68 Praesepe candidates have been detected, above a threshold of ~2x10^+28^erg/s (2x10^21^W), in the ~4degx4deg area of the cluster covered by the observations. 56 out of the 68 detected objects are cataloged as high probability Praesepe members.
ROSAT
Optical properties of X-ray detected Praesepe candidates Id X-ray number --- OtherId Optical identification number=1 KW: Klein-Wassink (1927) JC: Jones & Cudworth (1983) JS: Jones & Stauffer (1991) --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec Vmag V magnitude mag B-V B-V colour mag V-I V-I colour mag Proba Membership probability % n_Proba A 'p' means possible --- Sp Spectral type --- Notes Notes --- X-ray properties of the detected Praesepe candidates Id X-ray number --- n_Id Note --- ML Maximum Likelihood (ML) algorithm --- dRA Offset in right ascension arcsec dDE Offset in declination arcsec ct Counts ct/s e_ct rms uncertainty on counts (1 sigma error) ct/s Lx X-ray luminosity 10+22W e_Lx rms uncertainty on Lx (1 sigma error) 10+22W Lx/Lbol X-ray over bolometric luminosity --- l_HardR limit flag on HardR --- HardR Hardness ratio --- Undetected Praesepe candidates lying in the low sensitivity image region Name Star name --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec V V magnitude mag B-V B-V colour mag V-I V-I colour mag Proba Membership probability % Upct Upper limit on counts ct/s Lx Upper limit on X-ray luminosity (10^29^erg/s) 10+22W table2.tex LaTeX version of table2 table4.tex LaTeX version of table4 table5.tex LaTeX version of table5 Patricia Bauer CDS 1994 Nov 24 J_A+A_298_115.xml The jet-disk symbiosis II. Interpreting the Radio/UV correlations in quasars J/A+A/298/375 J/A+A/298/375 Jet-disk symbiosis II The jet-disk symbiosis II. Interpreting the Radio/UV correlations in quasars H Falcke M A Malkan P L Biermann Astron. Astrophys. 298 375 1995 1995A&A...298..375F accretion, accretion disks galaxies: active galaxies: jets galaxies: nuclei We investigate the correlation between the accretion disk (UV) luminosity and the radio core emission of a quasar sample, containing all PG quasars, also deriving empirical conversion factors from emission line luminosities to disk luminosities. This method allows us to investigate the radio properties of AGN on the absolute scale set by the accretion power. The tables contain the quasar (and radio galaxy) sample discussed in this paper (including the complete PG quasars sample) and give the derived `disk luminosities' of the UV-bump and 5GHz radio luminosities.
The quasar sample used in this paper Quasar Quasar ID number number=1 (n.1-n.87) is the PG sample with z<0.5 (n.88-n.113) is the rest of the PG sample (n.114-n.131) are quasars from Sun and Malkan 1989. An asterisk '*' marks quasars with new accretion disk fits and a dagger '+' marks the two quasars with strong variations between Mb and the UV --- Name Quasar IAU name --- z Redshift --- Class Class number=2 Q radio weak L radio loud S steep spectrum (alpha=<-0.5) F flat spectrum (alpha>-0.5) V variable spectrum P point source E extended emission D (double) lobe structure --- log(Ldisk) Logarithm of average disk luminosity 10-7W log(LdiskUV) Logarithm of disk luminosity derived from UV-bump fits 10-7W log(LdiskMb) Logarithm of disk luminosity derived from absolute blue magnitude 10-7W log(LdiskMv) Logarithm of disk luminosity derived from absolute magnitude of the continuum at 5500 A 10-7W log(LdiskeL) Logarithm of disk luminosity derived from emission lines seen in the optical spectrum 10-7W l_log(nu*L_nu_) Limit flag on radio luminosity --- log(nu*L_nu_) Logarithm of Radio luminosity of the core at 5GHz rest frame 10-7W l_f(c) Limit flag on ratio f(c) --- f(c) Radio of core flux to total flux at 5GHz rest frame % alpha Differential spectral index of fitted spectrum at 5GHz rest frame --- The FR II sample used in this paper Quasar Quasar ID number --- Name Quasar IAU name --- z Redshift --- Ldisk Logarithm of the disk luminosity derived by multiplying the lobe power calculated by Rawlings and Saunders (1991) 10-7W l_log(nu*L_nu_) Limit flag on radio luminosity --- log(nu*L_nu_) Logarithm of radio luminosity of the core at 5GHz rest frame 10-7W l_f(c) Limit flag on ratio f(c) --- f(c) Radio of core flux to total flux at 5GHz rest frame % alpha Differential spectral index of fitted spectrum at 5GHz rest frame --- Simona Mei CDS 1995 May 29 J_A+A_298_375.xml Deep infrared array photometry of galactic globular clusters: the main sequence of NGC 6171 J/A+A/298/461 J/A+A/298/461 Main sequence of NGC 6171 Deep infrared array photometry of galactic globular clusters: the main sequence of NGC 6171 F R Ferraro F Fusi Pecci P Montegriffo L Origlia V Testa Astron. Astrophys. 298 461 1995 1995A&A...298..461F globular clusters: individual (NGC 6171) Hertzsprung-Russell (HR diagram) infrared: stars stars: Population II techniques: photometric Deep J, K IR-array photometry for individual Main Sequence stars in NGC 6171 reaching K~18, about two magnitudes below the turnoff, is presented.
BVJK-photometry of 547 stars in NGC 6171 ID Identification number --- Bmag B-photometry mag Vmag V-photometry mag Jmag J-photometry mag Kmag K-photometry mag x x-coordinates (1 pixel=0.35 arcsec) pix y y-coordinates pix Patricia Bauer CDS 1994 Oct 24 J_A+A_298_461.xml Radio continuum observations of planetary nebula candidates from the northern hemisphere J/A+A/299/238 J/A+A/299/238 Radio observations of PN candidates Radio continuum observations of planetary nebula candidates from the northern hemisphere G C M Van de Steene S R Pottasch Astron. Astrophys. 299 238 1995 1995A&A...299..238V infrared: ISM: continuum planetary nebulae: general radio continuum: ISM We analyzed radio continuum observations of unidentified IRAS point sources with far IR colors that are typical of planetary nebulae. These IRAS-selected planetary nebula candidates are located outside the galactic bulge and were observed with the Westerbork Radio Synthesis Telescope. We have detected 20 new planetary nebulae out of 82 observed candidates. The detected sources are very close to the galactic plane. The detection rate is highest in that part of the color-color diagram, where planetary nebulae are expected to spend most time during their evolution. The radio and IR properties are compared with PN detected in the same way in the galactic bulge and with optical planetary nebulae which fulfill the same selection criteria. On average, the IR excess of the IRAS-selected and radio detected planetary nebula candidates is higher than for the optical planetary nebulae.
Far infrared data of the observed PN candidates in WSRT1 (Westerbork Synthesis Radio Telescope) Far infrared data of the observed PN candidates in WSRT2 Id Sequential number --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg F12 Far IR flux density at 12 {mu}m Jy F25 Far IR flux density at 25 {mu}m (upper limit for table3) Jy F60 Far IR flux density at 60 {mu}m Jy F100 Far IR flux density at 100 {mu}m Jy q_F12 Quality of F12 number=1 IRAS flux qualities: 3: good quality 2: moderate quality 1: upper limit --- q_F25 Quality of F25 number=1 IRAS flux qualities: 3: good quality 2: moderate quality 1: upper limit --- q_F60 Quality of F60 number=1 IRAS flux qualities: 3: good quality 2: moderate quality 1: upper limit --- q_F100 Quality of F100 number=1 IRAS flux qualities: 3: good quality 2: moderate quality 1: upper limit --- F12/F25 IRAS colour F12/F25 --- F25/F60 IRAS colour F25/F60 --- Tc Color temperature K FIR Total far infrared flux 10-13W/m2 rms rms error of the values of the fitted black body curve at 12, 25 and 60 {mu}m compared with the IRAS flux values at these wavelengths respectively Jy Patricia Bauer CDS 1995 Jan 16 J_A+A_299_238.xml A search for IRAS galaxies behind the Taurus molecular clouds. J/A+A/299/347 J/A+A/299/347 IRAS galaxies behind Taurus clouds A search for IRAS galaxies behind the Taurus molecular clouds. P Chamaraux I Kazes M Saito T Yamada T Takata Astron. Astrophys. 299 347 1995 1995A&A...299..347C galaxies: distances and redshifts infrared: galaxies large-scale structure of universe surveys We carried out a complete search for IRAS galaxies in the Taurus molecular cloud region at l=169deg to 177deg and b=-19deg to -12deg. We selected a total number of 36 galaxies and galaxy candidates and looked for the 21-cm H I line in 25 objects; we detected H I emission in five of them including one with previously unknown redshift. The spatial density of IRAS galaxies with cz=4000 to 6000km/s is lower in this region than in the adjacent regions at both sides along galactic longitude, where the Perseus supercluster and the Gemini-Monoceros filament are respectively located.
IRAS galaxies and galaxy candidates in the Taurus molecular cloud region Name IRAS name --- GLON Galactic longitude deg GLAT Galactic latitude deg S12 Flux at 12 {mu}m or density flux Jy n_S12 Note on S12 --- S25 Flux at 25 {mu}m or density flux Jy n_S25 Note on S25 --- S60 Flux at 60 {mu}m or density flux Jy S100 Flux at 100 {mu}m or density flux Jy n_S100 Note on S100 --- OptID Optical identification number=1 The 15 objects indicated by s?, s/neb, gal/neb, and blank belong to the objects with 'uncertain image' and FQ_12_=1 in Table 1. IRAS 04112+2432, 04251+2132, and 04444+2353 are, respectively, associated with CGCG 411.2+2432, UGC 3053, and UGC 3165 . --- cz Redshift velocity km/s n_cz Note on redshift velocity number=2 g: galactic *: we got the three unpublished redshift data denoted by * by private communication; they are larger than 7000 km/s --- r_cz References for redshift velocity number=3 References: a: Thonnard et al. 1978, AJ 83, 1564 b: Giovanelli & Haynes 1984, AJ 89, 758 c: Lu et al. 1990, ApJ 357, 388 d: Strauss et al. 1992, ApJS 83, 29 e: Strauss et al. 1994, private communication f: Takata et al. 1994b, in preparation --- Detect Detection --- table2.tex TeX version of table2 Patricia Bauer CDS 1994 Dec 08 J_A+A_299_347.xml OH/IR stars: near-infrared photometry, and discussion of the Mira-OH/IR sequence J/A+A/299/453 J/A+A/299/453 OH/IR stars photometry OH/IR stars: near-infrared photometry, and discussion of the Mira-OH/IR sequence J R D Lepine R Ortiz N Epchtein Astron. Astrophys. 299 453 1995 1995A&A...299..453L circumstellar matter infrared: stars stars: AGB and post-AGB stars: evolution This paper presents JHKL'M photometry of a new sample of OH/IR stars. These data are merged with similar observations collected in the literature in order to constitute a data base of near-infrared photometry for 400 OH/IR stars. After removing from this sample the objects that are unlikely to be AGB stars, we obtain a sequence of average OH/IR stars with increasing values of the colour index K-L'. A simple model of a star surrounded by a circumstellar shell is constructed in order to derive basic parameters such as luminosity, radius, stellar temperature, optical depth of the dust shell and mass loss rate. These parameters are found to vary smoothly along the sequence of OH/IR stars, and the K-L' colour is shown to describe almost completely the basic physical parameters of an OH/IR star. The metallicity affects the OH-peak separation, but does not play an important role in the definition of the other properties.
Near-infrared counterparts of OH/IR stars IRAS IRAS name --- Ref Reference number=1 00=this work; 01=Fouque et al. 1992; 02=Epchtein et al. 1990; 03=Guglielmo et al. 1993; 04=Epchtein & Nguyen-Quang-Rieu 1982; 05=Le Bertre 1987; 06=Le Bertre 1991; 07=Braz & Epchtein 1982; 08=Le Bertre et al. 1984; 09=Epchtein et al. 1980; 10=Epchtein & Lepine; 1981; 11=Le Bertre et al. 1984; 12=Epchtein et al. 1987; 13=Braz & Epchtein 1987; 14=Whitelock & Feast 1984; 15=Whitelock 1985; 16=Whitelock et al.1986; 17=Gaylard & Whitelock 1988; 18=Gaylard et al. 1989; 19=Whitelock et al. 1991; 20=Feast et al. 1983; 21=Glass 1988; 22=Glass 1986; 23=Glass 1978; 24=Persi et al. 1990; 25=Persi & Ferrari-Toniolo 1984; 26=Manchado et al. 1989; 27=Garcia-Lario et al. 1990; 28=Garcia-Lario et al. 1993; 29=van der Veen 1988; 30=Blommaert et al. 1993; 31=Blommaert 1992; 32=Willems & de Jong 1982; 33=Evans & Beckwith 1977; 34=Engels et al. 1981; 35=Schultz et al. 1976; 36=Werner et al. 1989; 37=Wilson et al. 1972; 38=Jones et al. 1982; 39=Jones et al. 1983; 40=Lawrence et al. 1990; 41=Fix & Mutel 1984; 42=Allen et al. 1977; 43=Gosnell et al. 1979; 44=Persson & Campbell 1988; 45=Nyman et al. 1993; 46=Le Bertre 1993 --- OtherRef Other reference number=1 00=this work; 01=Fouque et al. 1992; 02=Epchtein et al. 1990; 03=Guglielmo et al. 1993; 04=Epchtein & Nguyen-Quang-Rieu 1982; 05=Le Bertre 1987; 06=Le Bertre 1991; 07=Braz & Epchtein 1982; 08=Le Bertre et al. 1984; 09=Epchtein et al. 1980; 10=Epchtein & Lepine; 1981; 11=Le Bertre et al. 1984; 12=Epchtein et al. 1987; 13=Braz & Epchtein 1987; 14=Whitelock & Feast 1984; 15=Whitelock 1985; 16=Whitelock et al.1986; 17=Gaylard & Whitelock 1988; 18=Gaylard et al. 1989; 19=Whitelock et al. 1991; 20=Feast et al. 1983; 21=Glass 1988; 22=Glass 1986; 23=Glass 1978; 24=Persi et al. 1990; 25=Persi & Ferrari-Toniolo 1984; 26=Manchado et al. 1989; 27=Garcia-Lario et al. 1990; 28=Garcia-Lario et al. 1993; 29=van der Veen 1988; 30=Blommaert et al. 1993; 31=Blommaert 1992; 32=Willems & de Jong 1982; 33=Evans & Beckwith 1977; 34=Engels et al. 1981; 35=Schultz et al. 1976; 36=Werner et al. 1989; 37=Wilson et al. 1972; 38=Jones et al. 1982; 39=Jones et al. 1983; 40=Lawrence et al. 1990; 41=Fix & Mutel 1984; 42=Allen et al. 1977; 43=Gosnell et al. 1979; 44=Persson & Campbell 1988; 45=Nyman et al. 1993; 46=Le Bertre 1993 --- Catalog of near-infrared photometry of OH/IR stars IRAS IRAS name --- m_IRAS Multiplicity index on IRAS --- LON Longitude deg LAT Latitude deg Vlow Lowest velocity km/s Vhigh Highest velocity km/s Dist Distance kpc Kmag K magnitude mag J-H J-H colour mag H-K H-K colour mag K-L K-L colour mag L-M L-M colour mag Patricia Bauer CDS 1995 Feb 21 J_A+A_299_453.xml Red giants in open clusters: IV. NGC 3680 and IC 4651 J/A+A/299/53 J/A+A/299/53 Red giants in NGC 3680 and IC 4651 Red giants in open clusters: IV. NGC 3680 and IC 4651 J -C Mermilliod J Andersen B Nordstrom M Mayor Astron. Astrophys. 299 53 1995 1995A&A...299...53M binaries: spectroscopic individual:(IC 4651) open clusters and associations: individual (NGC 3680) stars: red giant Other papers in the series: Paper I =1989A&A...219..125M : NGC 2447, 2539, 2632, 6633 and 6940 Paper II =1989A&AS...79...11M : Binaries in NGC 2360, 2437, 2447, 5822, 5823 and 6475 Paper III =1990A&A...237...61M : NGC 2360, 2423, 5822, 6811 and IC 4756 Paper V =1996A&A...307...80M : NGC 2099. Paper VI =1997A&A...319..481M : Binaries in NGC 2489, 2567, 3033, 5822, 6134, 6664 and IC 2488
Radial velocity data for IC 4651 Radial velocity data for NGC 3680 ID Star number number=1 The numbering system used for NGC 3680 is from: Eggen O.J. 1969, Astrophys. J. 155,439 The numbering system used for IC 4651 is from: Lindoff U. 1972, Astron. Astrophys. Suppl. 7,231 For the identification of stars No 801 to 811 see the publication. --- HJD Heliocentric Julian Date d Comp Component of a double-lined binary --- RV Radial velocity km/s e_RV rms uncertainty on the radial velocity km/s Patricia Bauer CDS 1995 Feb 13 J.-C. Mermilliod <mermio@scsun.unige.ch> J_A+A_299_53.xml Beta Pictoris: Evidence of light variations J/A+A/299/557 J/A+A/299/557 Light variations on Beta Pic Beta Pictoris: Evidence of light variations A Lecavelier des Etangs M Deleuile A Vidal-Madjar R Ferlet C Nitschelm B Nicolet A M Lagrange-Henri Astron. Astrophys. 299 557 1995 1995A&A...299..557L circumstellar matter planetary systems stars: individual (beta Pic) We have analyzed {beta} Pictoris photometric measurements obtained from La Silla by the Geneva Observatory from 1975 to 1992. These data show evidence of variations in the brightness of the star, with no color dependency. Here, we demonstrate that the light variations are present on long as well as on short time scales. On a long time scale, we show that the apparent magnitude of {beta} Pictoris decreased by 0.011+/-0.004mag from 1979 to 1982. Moreover, when we consider all the measurements, the chance that there is no variation at all can be estimated to be less than 10^-4^. On short time scales there is a peculiar feature observed during about 30 days; the variations may be as high as 0.04mag magnitude. A maximum entropy reconstruction of the photometric data is tentatively proposed and some physical interpretations are presented.
Geneva photometry JD Julian date d q_Vmag Quality factor of the V magnitude --- Vmag V magnitude mag q_colours Quality factor of the colour indexes --- U-B U-B colour index mag V-B V-B colour index mag B1-B B1-B colour index mag B2-B B2-B colour index mag V1-B V1-B colour index mag G-B G-B colour index mag Simona Mei, Patricia Bauer CDS 1995 Feb 21 J_A+A_299_557.xml Is Sirius a triple star? J/A+A/299/621 J/A+A/299/621 Is Sirius a triple star? Is Sirius a triple star? D Benest J L Duvent Astron. Astrophys. 299 621 1995 1995A&A...299..621B binaries: general celestial mechanics, stellar dynamics stars: individual (alpha Cma) stars: low-mass, brown dwarfs Sirius has been discovered as double more than 130 years ago. From the beginning of our century up to now, observational as well as physical and dynamical indications lead to the hypothesis of the existence of a third body in the system. In this paper, we present recent orbital analysis of the binary Sirius A-B which, helped by numerical simulation of triple systems, strengthens the idea for the triplicity of Sirius: a tiny star could revolve in about 6 years around Sirius A. Finally, we discuss the possibility of direct detection for this suspected Sirius C.
Mean square Fourier analysis P Period yr Ax Fourier transforms Ax of O-Cx --- Ay Fourier transforms Ay of O-Cy --- Axy Mean of Ax, Ay --- Mean square sine function analysis (all data) P Period yr Ax Perturbation amplitude Ax of O-Cx --- Ay Perturbation amplitude Ay of O-Cy --- Axy Mean of Ax, Ay --- Observations of Sirius (1862-1979) Date Observation date yr Theta Position angle deg u_Theta Uncertainty flag on Theta --- Rho Separation angle arcsec u_Rho Uncertainty flag on Rho --- o_Theta Number of observations --- Name Observer name number=1 a = Aitken arc = Archer auw = Auwers b = van den Bos bar = Barnard bar = Barton baz = Baize bdg = Bond bea = Beal ber = Berman big = Bigourdan boo = Boothroyd brg = Boergen brh = Bruhns brn = Bruennow brs = Brown bru = Bruggencate btn = Burton btz = Bernewitz bu = Burnham chc = Chacornac com = Comstock cou = Couteau da = Dawes dic = Dick doo = Doolittle du = Duner eas = Eastman en = Engelmann fat = Fatou fbn = Brown fen = Fender fin = Finsen foe = Foester fox = Fox frs = Frisby fus = Fuss g = gcb=Giacobini gau = Gauchet gld = Gledhill gro = Greenwitch Observatory hei = Heintz hir = Hirst hl = Hall hld = Holden hln = Holden ho = Hough hu = Hussey hwe = Howe i = Innes j = Jonckheere jef = Jeffers jsp = Jessup jw = Wilson & Seabroke knp = Kniper knt = Knott kpz = Krumpholz l = Lewis ldb = Landbauer (?) lng = Lau Ling Fang loh = Lohse lsl = Lassel lv = Leavenworth ma = Mason mnl = McNeill mth = Marth nbg = Newburg neb = Neff & Burnham (?) nes = Newcomb o = Olsen ol = Olivier ole = Olevic pau = Pauscher pav = Pavel pec = Pechuele pei = Peirce pet = Peters phl = Phillips pop = Popovic pou = Pourteau prt = Pritchett r = Russell rab = Rabe roe = Roe rou = Rougier row = Rowg (doubtful observation) rut = Rutherford se = Secchi sea = Searle she = Sheberle ski = Skinner sm = Smith smw = Simonow stg = G.Struve stn = Stone stt = Otto Struve stv = Stevenson stv = Hermann Struve ttj = Tietjen tut = Tuttle upt = Upton vbs = van Biesbroeck vog = Vogel vou = Voute vys = Vyssotsky wak = Walker wal = Wallenquist wam = Wamer wat = Watson win = Winlock wnc = Winnecke wno = Washington Naval Observatory wor = Worley wz = Wirtz yng = Young. --- tables.tex Tables to be processed by plain TeX Patricia Bauer CDS 1994 Nov 28 J_A+A_299_621.xml Membership probabilities in the Pleiades field J/A+A/299/696 J/A+A/299/696 Pleiades field Membership probabilities Membership probabilities in the Pleiades field E Schilbach N Robichon J Souchay J Guibert Astron. Astrophys. 299 696 1995 1995A&A...299..696S astrometry open clusters and associations: individual (Pleiades) A catalogue of proper motions and photographic B,V magnitudes for stars up to B=19 mag within a region centered near Alcyone is presented. The catalogue is based on MAMA measurements of 8 plates taken with the Tautenburg Schmidt telescope. The survey includes ca. 14500 stars and covers a total field of about 9 square degrees. Membership probabilities, proper motions and B,V magnitudes are listed for 442 stars up to B=19 mag in the Pleiades field.
Position, proper motions, photometry and membership probabilities. Index Identification index --- n_Index See number=1 When '*' the stars have a membership probability based on their proper motion (ppm) larger than 50% and they match photometric criteria; when 'x' they have a ppm larger than 50% but they don't match photometric criteria; when '+' their ppm is smaller than 50% but they match photometric criteria; when there is an empty space their ppm is smaller than 50% and they don't match photometric criteria. --- RAh Right ascension (Eq. J2000.0, Ep. 1981.1) h RAm Right ascension (Eq. J2000.0, Ep. 1981.1) min RAs Right ascension (Eq. J2000.0, Ep. 1981.1) s DEd Declination (Eq. J2000.0, Ep. 1981.1) deg DEm Declination (Eq. J2000.0, Ep. 1981.1) arcmin DEs Declination (Eq. J2000.0, Ep. 1981.1) arcsec pmRA Proper motion in right ascension mas/yr e_pmRA Rms uncertainty on pmRA mas/yr pmDE Proper motion in declination mas/yr e_pmDE Rms uncertainty on pmDE mas/yr Bmag Magnitude B mag Vmag Magnitude V mag prob Membership probability % Name Other name number=2 bda: Base des Amas (Mermilliod J.-C. 1988, Bull. Inform. CDS 35,77; Mermilliod J.-C. 1992, Bull. Inform. CDS 40,115) sk: Stauffer J. et al. 1991, AJ 101,980 hcg: Haro G. et al. 1982, Boll. Inst. Tonantzintla 3,1 ak: Artyukhina N. et al. 1970, Trudy Shternberg Astr. Inst. 39,111 hhj: N.Hambly et al. 1993, A&AS 100,607. --- table1.tex Latex version of table1 Simona Mei CDS 1995 Feb 21 J_A+A_299_696.xml Stellar evolution of low and intermediate-mass-stars. II. Post-AGB evolution. J/A+A/299/755 J/A+A/299/755 Stellar evolution. II. Post-AGB Stellar evolution of low and intermediate-mass-stars. II. Post-AGB evolution. T Bloecker Astron. Astrophys. 299 755 1995 1995A&A...299..755B stars: AGB and post-AGB stars: evolution stars: mass-loss white dwarfs We present a set of evolutionary tracks for central stars of planetary nebulae in the range from 0.53 to 0.94M_{sun}_. These models are based on extensive stellar evolution calculations for initial masses between 1 and 7M_{sun}_ which have been carried out all the way from the main sequence through the AGB towards the stage of white dwarfs.
Data for hydrogen burning models Data for hydrogen burning models Data for helium burning models Minitial Initial mass solMass Mfinal Final mass solMass Age Post-AGB age yr log(Teff) Effective temperature K log(L) Luminosity solLum Patricia Bauer CDS 1995 Feb 21 Thomas Bloecker <tbloecker@aip.de> J_A+A_299_755.xml COYOTES II: Spot properties and the origin of photometric period variations in T Tauri stars J/A+A/299/89 J/A+A/299/89 COYOTES II COYOTES II: Spot properties and the origin of photometric period variations in T Tauri stars J Bouvier E Covino O Kovo E L Martin J M Matthews L Terranegra S C Beck Astron. Astrophys. 299 89 1995 1995A&A...299...89B V/73A : (HBC Catalogue, Lick Obs. Bull. 1111) accretion, accretion disks stars: activity stars: pre-main sequence stars: rotation We present the results of a new multi-site campaign (COYOTES II) to monitor the light variations of T Tauri stars (TTS) of the Taurus-Auriga dark cloud. The UBVRI light curves of 19 TTS were obtained over a two months period to search for rotational modulation by spots. We report new period detections for IQ Tau (6.25d), LkCa-3 (7.2d), and LkCa-14 (3.35d) and confirm previously detected periods for DF Tau (9.8d), DR Tau (9.0d), GM Aur (11.9d), and TAP 26 (2.58d). We also report tentative periods for CW Tau (8.2d), CY Tau (7.9d), HP Tau (5.9d), and XZ Tau (2.6d). No periods were found in the present data set for CI Tau, DG Tau, DQ Tau, GH Tau, RY Tau, Hubble 4, TAP 45, and TAP 57NW. Altogether, the results of this new campaign confirm the main conclusion of COYOTES I that classical T Tauri stars (CTTS) on average have longer rotational periods than weak-line TTS (WTTS). The present study also confirms that rotational modulation in WTTS is due to spots cooler than the photosphere and we show that the amplitude of the modulation primarily reflects the amount of areal coverage by spots. The amplitude of the light variations, and hence the spot size, is found to increase with both rotation rate and advancing spectral type, as expected if WTTS cool spots correspond to photospheric regions of strong dynamo-generated magnetic fields. Finally, combined with previous studies, these new results provide further evidence for temporal variations of the photometric periods of CTTS. Such variations seem to occur preferentially in CTTS whose rotational modulation is dominated by hot spots and we therefore argue that the observed period changes are linked to the magnetospheric accretion process rather than to surface differential rotation.
UBVRI photometry Name Star name --- HBC HBC number (Herbig Bell Catalog) --- JD Julian date d Vmag V magnitude mag B-V B-V colour mag U-B U-B colour mag V-R V-R colour mag V-I V-I colour mag Patricia Bauer CDS 1995 Jan 16 J_A+A_299_89.xml CCD photometry of the faint old open clusters ESO 96-SC04 and ESO 92-SC18 J/A+A/300/128 J/A+A/300/128 ESO 96-SC04 and ESO 92-SC18 photometry CCD photometry of the faint old open clusters ESO 96-SC04 and ESO 92-SC18 G Carraro A Vallenari S Ortolani Astron. Astrophys. 300 128 1995 1995A&A...300..128C open clusters and associations: general open clusters and associations: individual (ESO 96-SC04, ESO 92-SC18) We present deep CCD BV photometry in the central region of the faint open clusters ESO 96-SC04 and ESO 92-SC18. The color magnitude diagrams (CMD) here presented allows us to evaluate the clusters ages. We found an age of 5.0x10^9^yr for ESO 92-SC18 and 0.7x10^9^yr for ESO 96-SC04 on the Padova isochrones scale. Estimates of the reddening are given for both the target clusters and the distances of these objects are substantially revised. We conclude that these clusters belong to the old tail of the thin disk population, they are among the most distant known open clusters from the Sun and lie near the solar circle like the majority of the open clusters.
ESO 92-SC18 photometry ESO 96-SC04 photometry Seq Star identification (running) number --- Xpos X coordinate pix Ypos Y coordinate pix Vmag V magnitude mag B-V B-V colour mag Patricia Bauer, Francois Ochsenbein CDS 1995 Feb 21 UNKNOWN UNKNOWN The original files contained the magnitudes Vmag and B-V in E-format with 6 significant digits; these were converted into F5.2 values at CDS. J_A+A_300_128.xml The NOT gravitational lens survey for multiply imaged quasars J/A+A/300/323 J/A+A/300/323 NOT GL survey of multiply imaged quasars The NOT gravitational lens survey for multiply imaged quasars A O Jaunsen M Jablonski B R Pettersen R Stabell Astron. Astrophys. 300 323 1995 1995A&A...300..323J dark matter gravitaional lensing large-scale structure of universe quasars: general A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.
The complete observational list of the 168 QSOs in the NOT sample QSO QSO identification, where the first letter(s) indicates the origin: H: from Hazard, HS: from Reimers (Hamburg Sternwarte) others from the Veron catalogue --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Filter Filter types --- FWHM Seeing (FWHM) arcsec z Redshift z of the QSO --- Vmag V-band magnitude of the QSO as estimated from our data or tabulated in other QSO catalogues. The QSOs with no previously measured magnitude were estimated by comparing them to QSOs on other CCD frames (for a similar exposure time) These estimated magnitudes are marked by an asterisk (*) and have errors up to +/- 0.5 mag mag Dmag Magnitude difference between closest companion with weaker apparent brightness and within 5 arcsec of QSO mag Sep Separation of closest companion with weaker apparent brightness and within 5 arcsec of QSO arcsec GLc See Note number=1 1 indicates that the QSO is treated as a possible GL candidate while 2 indicates that the object is elongated, diffuse or otherwise especially interesting. The latter objects are not treated as GL candidates in the present analysis, but should be further analysed in future work. --- Note See Note number=2 1 indicates that there are one or more PSFs and the QSO is not elongated 2 indicates that the QSO appears elongated (this is sometimes due 3 indicates that there are no PSFs other than the QSO in the image to bad tracking) --- Patricia Bauer CDS 1995 Feb 17 J_A+A_300_323.xml BH 176 and AM-2: globular or open clusters ? J/A+A/300/726 J/A+A/300/726 BH 176 and AM-2 BH 176 and AM-2: globular or open clusters ? S Ortolani E Bica B Barbuy Astron. Astrophys. 300 726 1995 1995A&A...300..726O globular clusters: individual (BH 176) Hertzsprung-Russell (HR diagram) open clusters and associations: individual (AM-2) We have obtained VI photometry for two low Galactic latitude star clusters: BH 176 and AM-2, using the 2.2m and the 3.5m NTT telescopes at ESO. Their VI colour-magnitude diagrams reveal that: BH 176 may be a globular cluster, or a border line object between a globular cluster and a disk cluster, showing a red horizontal branch and an extended red giant branch. We estimate E(B-V)=0.77 and d_{sun}_=13.4kpc. AM-2 appears to be an intermediate age open cluster, for which a reddening E(B-V)=0.44 and d_{sun}_=12.4kpc are estimated. It is located in the outer regions of the Galactic disk.
AM-2 coordinates, V magnitude and V-I colour BH 176 coordinates, V magnitude and V-I colour No Star number --- X X coordinate pix Y Y coordinate pix Vmag V magnitude mag V-I (V-I) colour mag Patricia Bauer CDS 1995 Jan 06 J_A+A_300_726.xml Spectroscopic analyses of metal-poor stars. II. The evolutionary stage of subdwarfs. J/A+A/300/751 J/A+A/300/751 Metal-poor stars spectroscopy. II Spectroscopic analyses of metal-poor stars. II. The evolutionary stage of subdwarfs. M Axer K Fuhrmann T Gehren Astron. Astrophys. 300 751 1995 1995A&A...300..751A stars: distances stars: evolution stars: fundamental parameters stars: kinematics subdwarfs Models of post-main sequence stellar evolution of VandenBerg & Bell have been applied to determine spectroscopic masses and distances for metal-poor stars. Careful consideration of the most important error sources published in more recent papers such as VandenBerg for the first time allow us to draw firm statistical conclusions. It is shown that the evolutionary calculations qualitatively fit to the observed stellar parameters whereas quantitatively they predict too high ages for metal-poor stars. As an important result we confirm that evolutionary sequences need to be calibrated with respect to their metal abundance in order to use their absolute predictions of temperature and luminosity. In our spectroscopic analyses the strong dependence between surface gravity and abundances determined from Fe I lines restricts the accuracy of Fe abundances in subgiants to 0.1 dex at best. The most remarkable result of our evolutionary and kinematic investigations of halo stars refers to the large fraction of slightly evolved subgiants among the so-called subdwarfs. Since conventional photometric approaches often assume that the great majority of metal-poor stars are dwarfs this results in distances that are systematically too low for their samples.
Fundamental stellar parameters of the program stars HD HD number --- G Giclas number --- Name Other name --- Teff Effective temperature for LTE assumption K logg1 Surface gravity for LTE assumption cm/s2 [Fe/H]1 Metallicity for LTE assumption Sun Class Subdivision in three classes of LTE assumption --- Dlogg Non-LTE correction in logg cm/s2 D[Fe/H] non-LTE correction in [Fe/H] Sun logg2 Surface gravity for non-LTE assumption cm/s2 e_logg1 rms uncertainty on log g1 (LTE value) cm/s2 [Fe/H]2 Metallicity for non-LTE assumption Sun e_[Fe/H]1 rms uncertainty on [Fe/H]1 (LTE value) Sun Stellar parameters derived from spectroscopy assuming LTE Stellar parameters derived from spectroscopy including non-LTE corrections HD Hd number --- G Giclas number --- Name Other name --- D(log(Teff)) Temperature corrections necessary for individual adjustment to the metal abundance K BC Bolometric correction mag Mass Mass solMass e_Mass rms uncertainty on Mass solMass plx Spectroscopic parallax arcsec e_plx rms uncertainty on plx arcsec Dist Distance pc e_Dist rms uncertainty on distance pc MV Absolute visual magnitude mag e_MV rms uncertainty on MV mag Mbol Bolometric magnitude mag e_Mbol rms uncertainty on Mbol mag Galactic velocities HD HD number --- G Giclas number --- Name Other name --- RV Radial velocity km/s pmRA proper motion in right ascension s pmDE Proper motion in declination arcsec U1 U velocity for LTE assumption km/s V1 V velocity for LTE assumption km/s W1 W velocity for LTE assumption km/s Vgal1 Galactic velocity for LTE assumption km/s e_Vgal1 rms uncertainty on Vgal1 km/s U2 U velocity for non-LTE assumption km/s V2 V velocity for non-LTE assumption km/s W2 W velocity for non-LTE assumption km/s Vgal2 Galactic velocity for non-LTE assumption km/s e_Vgal2 rms uncertainty on Vgal2 km/s Patricia Bauer CDS 1995 Jan 05 J_A+A_300_751.xml CCD Photometry of the Young Association NGC 1962-65-66-70 in the Large Magellanic Cloud J/A+A/301/396 J/A+A/301/396 Photometry of NGC 1962-65-66-70 CCD Photometry of the Young Association NGC 1962-65-66-70 in the Large Magellanic Cloud J M Will A Vazquez A Feinstein W Segeewiss Astron. Astrophys. 301 396 1995 1995A&A...301..396W galaxies: star clusters Magellanic Clouds open clusters and associations: individual (NGC 1962, NGC 1965) open clusters and associations: individual (NGC 1966, NGC 1970) stars: individual (HDE 269551) stars: luminosity function, mass function We present CCD data in the Johnson passbands B and V of the young association NGC 1962-65-66-70 in the Large Magellanic Cloud.
Photometry of 1920 stars in the field of NGC 1962-65-66-70 in the B and V passbands. Star Star running number --- Xpos position on CCD frame as given by DAOPHOT pix Ypos position on CCD frame as given by DAOPHOT pix Vmag Calibrated V magnitude of star mag B-V Calibrated B-V colour of star mag e_Vmag Rms uncertainty on V magnitude mag e_B-V Rms uncertainty on B-V colour mag Simona Mei CDS 1995 Apr 03 J_A+A_301_396.xml EROS variable stars: fundamental-mode and first-overtone Cepheids in the bar of the Large Magellanic Cloud. J/A+A/303/137 J/A+A/303/137 EROS Variables: Cepheids in the bar of LMC EROS variable stars: fundamental-mode and first-overtone Cepheids in the bar of the Large Magellanic Cloud. J -P Beaulieu P Grison W Tobin J D Pritchard R Ferlet F Lepeintre A Vidal-Madjar E Maurice L Prevot C Gry J Guibert O Moreau F Tajhamady E Aubourg P Bareyre C Coutures M Gros B Laurent M Lachieze-Rey E Lesquoy C Magneville A Milsztajn L Moscoso F Queinnec C Renault J Rich M Spiro L Vigroux S Zylberajch R Ansari F Cavalier M Moniez Astron. Astrophys. 303 137 1995 1995A&A...303..137B Cepheids Magellanic Clouds surveys We present CCD phase-binned light curves at 490nm for 97 Cepheid variable stars in the bar of the LMC. The photometry was obtained as part of the French EROS project and has excellent phase coverage, permitting accurate decomposition into Fourier components. We identify as `sinusoidal' or s-Cepheids those stars with periods less than 5.5d and small second-harmonic components. These stars comprise ~30% of our sample and most form a sequence ~1mag brighter than the LMC classical Cepheids in the period-luminosity diagram. They are also generally bluer and have lower-amplitude light curves. We infer that the s-Cepheids are first-overtone pulsators because, when their periods are converted to expected fundamental-mode values, they obey a common period-luminosity-colour relation with classical Cepheids. This also confirms the reality of the colour term in the Cepheid period-luminosity-colour relation. Further, the blue edge of the classical Cepheid instability strip agrees well with the theoretical calculations for the fundamental mode made by Chiosi et al. 1993 (=1993ApJS...86..541C) for the Hertzsprung-Russell and period-luminosity diagrams, but we find that our observed s-Cepheids are >0.2mag brighter and bluer than the Chiosi et al. predictions for the first-overtone. We identify a number of features in plots of our stars' Fourier-component amplitude ratios and phase differences. These features have been identified with resonances between different pulsation modes. In the LMC we find these features seem to occur at periods very similar to Galactic ones for classical Cepheids, but at different periods for s-Cepheids. We discover a double-mode Cepheid in the LMC, for which P(first overtone)/P(fundamental)=0.710+/-0.001, very similar to observed ratios for Galactic double-mode Cepheids.
97 LMC bar Cepheids EROS EROS number --- HV HV number (Harvard Variable) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec P Period d Type See Note number=1 A: Classical light curves B: s-Cepheids C: anomalous types D: double mode Cepheids E: intermediate objects in the R_21_-P plane --- BE B_E_ magnitude mag RE R_E_ magnitude mag R2/1 Ratio of second harmonic; see note number=2 Observed magnitude are decomposed in Fourier with X = X0 + X1 cos( (2{pi}/P)(t-t_0_) + Phi1) + ... + Xk cos(k(2{pi}/P)(t-t_0_) + Phik) + ... Ratios are defined by Rk/1 = Xk/X1 (k>1) --- R3/1 Ratio of third harmonic; see note number=2 Observed magnitude are decomposed in Fourier with X = X0 + X1 cos( (2{pi}/P)(t-t_0_) + Phi1) + ... + Xk cos(k(2{pi}/P)(t-t_0_) + Phik) + ... Ratios are defined by Rk/1 = Xk/X1 (k>1) --- Phi2/1 Phase difference; see note number=3 Phase differences are defined by Phik/1 = Phik - k . Phi1 (k>1) --- Phi3/1 Phase difference; see note number=3 Phase differences are defined by Phik/1 = Phik - k . Phi1 (k>1) --- e_BE Error on BE magnitude mag e_RE Error on RE magnitude mag e_R2/1 Error on R2/1 parameter --- e_R3/1 Error on R3/1 parameter --- e_Phi2/1 Error on phase difference Phi2/1 --- e_Phi3/1 Error on phase difference Phi3/1 --- Remarks Remarks --- Simona Mei CDS 1995 Dec 07 J_A+A_303_137.xml The 654-1046nm line spectrum of the planetary nebula NGC 7027 J/A+A/303/175 J/A+A/303/175 Line spectrum of NGC 7027 The 654-1046nm line spectrum of the planetary nebula NGC 7027 J -P Baluteau A Zavagno C Morisset D Pequignot Astron. Astrophys. 303 175 1995 1995A&A...303..175B atomic data line: identification planetary nebulae: individual (NGC 7027) Deep CCD spectra of the planetary nebula NGC 7027, taken over the range 654-1046nm at a spectral resolution of the order of 0.1nm, are presented. About 465 different lines are detected and intensities are provided for 405 features. A total of 680 emission lines is considered.
Lines in the spectrum of NGC 7027 Id Line identification number=1 An 'X' indicates unidentified lines. An '{' in first column indicates several possible identification lines for the same observed line. --- LamTheo Theoretical wavelength nm n_LamTheo '}' indicates several identification lines for the same observed wavelength '*' indicates a note on [FeIV] --- u_LamTheo Uncertainty flag on LamTheo --- LamObs Observed wavelength nm o_LamObs Number of independent measurements --- Ilam/Ibeta Line intensity in I(Hbeta)/10+4 10-4 e_Ilam/Ibeta rms uncertainty on 10+4F/Ibeta % Com Comments number=2 The abbreviations mean: (a) in the wing of a nearby strong line (b) difficult continuum level estimate (c) blend with nearby lines (d) broad feature --- table2.tex LaTeX version of table2 Patricia Bauer CDS 1995 Mar 07 J_A+A_303_175.xml Cosmological evolution and large scale structures of radio galaxies and quasars J/A+A/303/420 J/A+A/303/420 Radio galaxies and quasars Cosmological evolution and large scale structures of radio galaxies and quasars K T Chyzy S Zieba Astron. Astrophys. 303 420 1995 1995A&A...303..420C Active gal. nuclei QSOs Radio sources Redshifts cosmology: observations galaxies: active quasars: general radio continuum: galaxies The simple unification scheme of powerful radio galaxies and quasars, based entirely on the orientation dependent effects, has been confronted with the observed radio structures for 152 radio galaxies and 173 steep spectrum quasars. Contrary to the scheme's prediction, the cosmological evolution of geometrical parameters describing the large scale structure of these two types of radio sources are different.
The sample of 152 radio galaxies The sample of 173 quasars Name Source name --- z Redshift --- logP 1.4 GHz spectral luminosity W/Hz Q Arms ratio number=1 Ratio of the distances of hot spots from the core --- M Misalignment number=2 Ratio of the displacement of the core from the radio source axis to the source linear size --- L Linear size kpc Notes References to radio data number=3 3C - Spinrad et al. (1985); AL - Alexander and Leahy (1987); Ba - Barthel and Miley (1988); BB - Burnst et al. (1984); Be - Bedford et al. (1981); BM - Barthel et al. (1988); B2 - Ragora et al. (1986); Dja - Djorgovski et al. (1987); Djb - Djorgovski et al. (1988); Fe - Feigelson et al. (1984); GB2 - Machalski and Maslowski (1982); GB3 - Machalski and Condon (1983a); GB4 - Machalski and Condon (1983b); GB5 - Machalski and Condon (1985); GC - Garrington et al. (1991); GH - Gower and Hutchings (1984); Gu - Gunn et al. (1981); Hi - Hintzen et al. (1983); Hu - Hutchings et al. (1988); JB - Jagers et al. (1982); JP - Jenkins et al. (1977); La - Laing (1981); LB - Lonsdale and Barthel (1987); Lo - Longair (1975); Mc - Macklin (1981) and references therein; MH - Miley and Hartsuijker (1978); NB - Neff and Brown (1984); OP - Owen and Pushell (1984); Pe - Pedelty et al. (1989); PH - Pooley and Henbest (1974); PKS - Dunlop et al. (1989); RA - Rudnick and Adams (1979); RP - Riley and Pooley (1975); RW - Riley and Warner (1990); SB - Stocke et al. (1985). --- Simona Mei CDS 1995 May 15 Krzysztof Chyzy <chris@oa.uj.edu.pl> J_A+A_303_420.xml Ultraviolet observations of galaxies in nearby clusters. III. Star-forming galaxies in the Coma Cluster J/A+A/303/661 J/A+A/303/661 Star-forming galaxies in the Coma Cluster Ultraviolet observations of galaxies in nearby clusters. III. Star-forming galaxies in the Coma Cluster J Donas B Milliard M Laget Astron. Astrophys. 303 661 1995 1995A&A...303..661D galaxies: individual (Coma cluster) galaxies: interactions galaxies: photometry ultraviolet: galaxies In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.
Galaxies data NFOCA FOCA identification number --- NGMP GMP identification number number=1 GMP: Godwin et al. 1983. --- RAh Right ascension (1950) number=2 Corrisponded to the galaxy identified with the UV source. h RAm Right ascension (1950) number=2 Corrisponded to the galaxy identified with the UV source. min RAs Right ascension (1950) number=2 Corrisponded to the galaxy identified with the UV source. s DEd Declination (1950) number=2 Corrisponded to the galaxy identified with the UV source. deg DEm Declination (1950) number=2 Corrisponded to the galaxy identified with the UV source. arcmin DEs Declination (1950) number=2 Corrisponded to the galaxy identified with the UV source. arcsec n_UVmag When '*' source is close to UV bright stars and her flux is only estimated --- UVmag UV magnitude at 2000 A mag UV-b UV - b colour index, when b is the magnitude given in GMP number=1 GMP: Godwin et al. 1983. mag RVel Heliocentric radial velocity in PGC number=3 PGC: Paturel G. et al. 1989. For five galaxies (NFOCA=2009, 829, 728, 736 and 701) the heliocentric radial velocity is taken in Caldwell N., Rose J.A., Sharples R.M., Ellis R.S., Bower R.G., 1993, AJ, 106, 473. km/s Id Identification in PGC number=3 PGC: Paturel G. et al. 1989. For five galaxies (NFOCA=2009, 829, 728, 736 and 701) the heliocentric radial velocity is taken in Caldwell N., Rose J.A., Sharples R.M., Ellis R.S., Bower R.G., 1993, AJ, 106, 473. --- The UV sources identified with two closely unresolved galaxies NFOCA FOCA identification number --- RAh Right ascension (1950)(see Note (2) in table1) h RAm Right ascension (1950)(see Note (2) in table1) min RAs Right ascension (1950)(see Note (2) in table1) s DEd Declination (1950)(see Note (2) in table1) deg DEm Declination (1950) (see Note (2) in table1) arcmin DEs Declination (1950) (see Note (2) in table1) arcsec UVmag UV magnitude at 2000 A mag Id1 GMP identification of the first candidate galaxy --- Id2 GMP identification of the second candidate galaxy --- UVmag-b UV - b colour index, when b is the magnitude given in GMP (see Note (1) in table1) mag RVel Heliocentric radial velocity in PGC (see Note (3) in table1) km/s Id Identification in PGC (see Note (3) in table1) --- Simona Mei CDS 1995 May 12 J_A+A_303_661.xml On the status of planetary nebulae with WR-type nuclei J/A+A/303/893 J/A+A/303/893 Planetary nebulae with WR-type nuclei On the status of planetary nebulae with WR-type nuclei S K Gorny G Stasinska Astron. Astrophys. 303 893 1995 1995A&A...303..893G planetary nebulae: general stars: Wolf-Rayet A recent systematic search of Wolf-Rayet features in the spectra of Galactic planetary nebulae has increased the list of objects that are known to have WR-type nuclei to about 50. We have compared their nebular properties with those of the other planetary nebulae in the Galaxy.
Properties of planetary nebulae with WR-type central stars PNG PNG designation --- Name Name --- Sp Spectral class of the central star --- MType Morphological type number=1 E elliptical nebulae B bipolar nebulae P point symmetric nebulae I irregular nebulae s structure presence m multishell presence : general morphological type or structure/multishell presence uncertainty sign (colon) --- RefSou References to images sources number=2 1 Chu et al. (1987) 2 Schwarz et al. (1992) 3 Bassgen & Bremer (1993) 4 Kaler et al. (1991) 5 Koppen et al. (1991) 6 Perinotto (1991) 7 Ratag (1991) 8 Walton et al. (1993) 9 Cuisinier - private communication 10 Kingsburgh & Barlow (1994) 11 Weinberger (1989) 12 Tamura & Shibata (1990) 13 Hutsemekers & Surdej (1989) 14 Bianchi (1992) 15 Leuenhagen et al. (1993) 16 de Freitas Pacheco et al. (1993) --- l_He/H Upper/lower He/H ratio limit sign --- He/H He/H abundance ratio --- u_He/H He/H ratio uncertainty flag --- N/O N/O abundance ratio --- u_N/O N/O ratio uncertainty flag --- C/O C/O abundance ratio --- u_C/O C/O ratio uncertainty flag --- RefAbun Reference to abundances number=2 1 Chu et al. (1987) 2 Schwarz et al. (1992) 3 Bassgen & Bremer (1993) 4 Kaler et al. (1991) 5 Koppen et al. (1991) 6 Perinotto (1991) 7 Ratag (1991) 8 Walton et al. (1993) 9 Cuisinier - private communication 10 Kingsburgh & Barlow (1994) 11 Weinberger (1989) 12 Tamura & Shibata (1990) 13 Hutsemekers & Surdej (1989) 14 Bianchi (1992) 15 Leuenhagen et al. (1993) 16 de Freitas Pacheco et al. (1993) --- ExpVel 2*expansion velocity km/s u_ExpVel Expansion velocity uncertainty flag --- r_ExpVel Reference to expansion velocity number=2 1 Chu et al. (1987) 2 Schwarz et al. (1992) 3 Bassgen & Bremer (1993) 4 Kaler et al. (1991) 5 Koppen et al. (1991) 6 Perinotto (1991) 7 Ratag (1991) 8 Walton et al. (1993) 9 Cuisinier - private communication 10 Kingsburgh & Barlow (1994) 11 Weinberger (1989) 12 Tamura & Shibata (1990) 13 Hutsemekers & Surdej (1989) 14 Bianchi (1992) 15 Leuenhagen et al. (1993) 16 de Freitas Pacheco et al. (1993) --- MLRate Mass loss rate 10-6solMass/yr r_MLRate Reference to mass loss rate number=2 1 Chu et al. (1987) 2 Schwarz et al. (1992) 3 Bassgen & Bremer (1993) 4 Kaler et al. (1991) 5 Koppen et al. (1991) 6 Perinotto (1991) 7 Ratag (1991) 8 Walton et al. (1993) 9 Cuisinier - private communication 10 Kingsburgh & Barlow (1994) 11 Weinberger (1989) 12 Tamura & Shibata (1990) 13 Hutsemekers & Surdej (1989) 14 Bianchi (1992) 15 Leuenhagen et al. (1993) 16 de Freitas Pacheco et al. (1993) --- Morphological types of the non-WR planetary nebulae PNG PNG designation --- Name Name --- Mtype Morphological type --- RefSou References to images sources number=1 1 Chu et al. (1987) 2 Schwarz et al. (1992) 3 Bassgen & Bremer (1993) --- Simona Mei CDS 1995 May 15 Gorny S.K. <skg@ncac.torun.pl> J_A+A_303_893.xml Toward a consistent model of the B0.5IVe + sdO binary phi Per J/A+A/304/235 J/A+A/304/235 UBV Photometry of phi Per Toward a consistent model of the B0.5IVe + sdO binary phi Per H Bozic P Harmanec J Horn P Koubsky G Scholz D McDavid A -M Hubert H Hubert Astron. Astrophys. 304 235 1995 1995A&A...304..235B Photometry, UBV Stars, variable binaries: spectroscopic stars: emission-line, Be stars: fundamental parameters stars: individual (phi Per) A detailed analysis of a very rich collection of spectroscopic and photometric observations of the bright Be star {phi} Per (HR 496, or HD 10516, 2000 position: 01 43 39.4 +50 41 20) is presented. Earlier reports that {phi} Per is a double-lined spectroscopic binary consisting of two emission-line objects are confirmed.
phi Per HD 10516 01 43 39.4 +50 41 20
UBV photometry of Phi Per All-sky UBV photometry of Phi Per HJD Julian date d Weight Weight --- Vmag V magnitude mag e_Vmag rms uncertainty on V magnitude mag Bmag B magnitude mag e_Bmag rms uncertainty on B magnitude mag Umag U magnitude mag e_Umag rms uncertainty on U magnitude mag B-V B-V colour index mag U-B U-B colour index mag Station Observing station and instruments number=1 1: Hvar, Croatia, 0.65-m 10: Kitt Peak, USA, 0.40-m 15: Phoenix, Mt.Hopkins, Arizona, USA, APT-10 0.254-m 21: Berlin-Babelsberg, Germany, 0.30-m refractor, Na diode 22: Berlin-Babelsberg, Germany, 0.30-m refractor, Rb diode 23: Catalina, Italy, orig. 1P21 24: McDonald, USA, 0.33-m 25: Uppsala, Sweden, double refl. 26: Haute Provence, France, 0.60-m 27: Bologna, Loiano, Italy, 0.60-m 28: Corialiotis Obs., USA 29: Glenlea, Manitoba, Canada, 0.35-m 30: San Pedro Martir,Mexico, 0.84 & 1.5-m 31: Steward obs. --- Simona Mei CDS 1995 May 15 UNKNOWN UNKNOWN * 15-May-1995: First version * 23-Jan-1996: table6a corrected, following the message from Petr Harmanec <hec@sunstel.asu.cas.cz>: "Recently, I found a round-off error in our data archiving programs. Table 6 of the study of Phi Per (Bozic et al. 1995 A&A 304, 235) has, therefore, slightly incorrect Julian dates." J_A+A_304_235.xml Metallicities and carbon abundances of 40 field red supergiants in the Small Magellanic Cloud J/A+A/304/347 J/A+A/304/347 40 field red supergiants in the SMC Metallicities and carbon abundances of 40 field red supergiants in the Small Magellanic Cloud M T Meliani B Barbuy T Richtler Astron. Astrophys. 304 347 1995 1995A&A...304..347M Spectrophotometry galaxies: abundances Magellanic Clouds stars: abundances Low-resolution spectra (~5A) for 40 red supergiants in the Small Magellanic Cloud were compared with synthetic spectra, and their metallicities were derived. A mean metallicity of [Fe/He]=-0.71 is found for 38 stars cooler than T_eff_<4500K. Using the stellar parameters derived, the carbon abundances were determined by comparing synthetic spectra at the G-band region to the observed spectra. A mean {epsilon}(C)=7.85 is found, clearly higher than the low values suggested in the literature for the H II regions.
List of programme stars Name Name of the star number=1 the following acronyms are used: [S78d] refers to Sanduleak 1978, partially published by Humphreys (1979ApJ...231..384H) PMMR refers to Prevot, Martin, Maurice, Rebeirot, Rousseau (1983A&AS...53..255P) --- Variable Variable name --- RAh Right Ascension 1975 (hours) h RAm Right Ascension 1975 (minutes) min RAs Right Ascension 1975 (seconds) number=2 non-accurate positions (0.1min accuracy in RA, 1arcmin in DE) have blank DEs (arcsec declination) values. s DE- Declination 1975 (sign) --- DEd Declination 1975 (degrees) deg DEm Declination 1975 (minutes) arcmin DEs Declination 1975 (seconds) number=2 non-accurate positions (0.1min accuracy in RA, 1arcmin in DE) have blank DEs (arcsec declination) values. arcsec SpType Spectral type --- Bmag B magnitude (from SIMBAD) mag Vmag V magnitude (from SIMBAD) mag File Name of file containing the spectrum --- Relative spectrum of PMMR 5 Relative spectrum of PMMR 10 Relative spectrum of PMMR 12 Relative spectrum of PMMR 27 Relative spectrum of PMMR 28 Relative spectrum of PMMR 43 Relative spectrum of PMMR 47 Relative spectrum of PMMR 48 Relative spectrum of PMMR 56 Relative spectrum of PMMR 62 Relative spectrum of PMMR 89 Relative spectrum of PMMR 102 Relative spectrum of PMMR 106 Relative spectrum of PMMR 118 Relative spectrum of PMMR 119 Relative spectrum of PMMR 122 Relative spectrum of PMMR 123 Relative spectrum of PMMR 126 Relative spectrum of PMMR 131 Relative spectrum of PMMR 134 Relative spectrum of [S78d] 13 Relative spectrum of [S78d] 15 Relative spectrum of [S78d] 21 Relative spectrum of [S78d] 30 Relative spectrum of [S78d] 36 Relative spectrum of [S78d] 37 Relative spectrum of [S78d] 39 Relative spectrum of [S78d] 44 Relative spectrum of [S78d] 47 Relative spectrum of [S78d] 51 Relative spectrum of [S78d] 52 Relative spectrum of [S78d] 58 Relative spectrum of [S78d] 67 Relative spectrum of [S78d] 71 Relative spectrum of [S78d] 78 Relative spectrum of [S78d] 90 Relative spectrum of [S78d] 91 Relative spectrum of [S78d] 92 Relative spectrum of [S78d] 96 Relative spectrum of [S78d] 100 Lam Wavelength (Angstroems) 0.1nm I Relative spectrum at wavelength Lam --- fig1a.ps Observed spectra for P106, P56, P10, H100, H44, P62, P102, P43, H37, P28 fig1b.ps Observed spectra for P48, P134, P123, H91, P89, H71, H67, H21, P47, P12 fig1c.ps Observed spectra for H58, H47, P131, P119, H92, P118, P122, H39, H36, H96 fig1d.ps Observed spectra for H30, H78, H51, P27, H15, H52, H90, P5, H13, P126 Simona Mei, Francois Ochsenbein CDS 1996 Jan 24 UNKNOWN UNKNOWN * PostScript figures were received at CDS in July 1995, and ascii tables in January 1996. The file "stars.dat" was added at CDS in January 1996. J_A+A_304_347.xml Pulsation and binarity in Beta Cephei Stars. II. 16 Lac J/A+A/304/406 J/A+A/304/406 Photometry and radial velocities of 16 Lac Pulsation and binarity in Beta Cephei Stars. II. 16 Lac E Chapellier J M Le Contel D Le Contel J P Sareyan J C Valtier Astron. Astrophys. 304 406 1995 1995A&A...304..406C binaries: close stars: individual (16 Lac) stars: pulsation stars: variables: other Photometric and spectroscopic observations of the {beta} Cephei star 16 Lacertae obtained in 1983 and 1984 are presented and analysed. Using all the published maxima we have computed ephemerides for each of the three pulsational modes. No period variation is detected from 1950 to 1983. In order to identify the pulsational modes corresponding to the three main periods of 16 Lac we have applied different methods based on photometric and radial velocity variations. All give the same results: the mode corresponding to the largest amplitude P_1_ (016917d) is radial, P_2_ (017079d) is a nonradial mode of degree l=2. For P_3_ (018171d) the results are more dubious, but P_3_ is probably a l=1 nonradial mode. We have also studied the interaction between pulsation and binarity in 16 Lac. We confirm the existence of a resonance phenomenon between the radial and nonradial modes: the ratios between the beat frequencies of the pulsational modes and the orbital frequency are close but significantly different from simple rational numbers. According to Kato (1974) that means that the nonradial modes might be excited or at least enhanced by tidal effects. They would have been selected among all the possible modes because their ability to be resonant with the radial mode. The photometric amplitude of P_3_ in both filters appears to be variable from night to night in correlation with the orbital phase but despite its rapid and irregular fluctuations, the P_3_ amplitude stayed in constant average over 80 years. The present observations confirm the decrease of P_1_ and P_2_ amplitudes since 1950 but an analysis of older radial velocity data shows that the amplitude of the P_1_ mode went through a maximum around the middle of the century before the observed decrease of the last thirty years.
HR 8725 16 Lac HD 216916 22 56 23.5 +41 36 14
Photometric data Date Date "DD/MM/YY" Filter Filter number=1 filter 4 (UV): Lambda= 3513 A, DeltaLambda= 94 A filter 5 (blue): Lambda= 4766 A, DeltaLambda= 112 A; Sareyan et al. 1976. --- JD Julian day d DMag Magnitude difference between 16 Lac and 2 And mag Radial velocity data JD Julian day d RV Radial velocity of 16 Lac. km/s Simona Mei CDS 1995 Jun 07 J_A+A_304_406.xml A pulsating star inside Eta Carinae I. Light variations 1992-1994 J/A+A/304/415 J/A+A/304/415 uvby-Hbeta photometry of Eta Car 1992-94 A pulsating star inside Eta Carinae I. Light variations 1992-1994 A M van Genderen C Sterken M De Groot O Stahl J Andersen M I Andersen J A R Caldwell B Casey R Clement W J B Corradi J Cuypers H Debehogne J M Garcia de Maria H Joench-Soerensen L P R Vaz S Stefl J Suso Lopez D Beele I M M G Eggenkamp K -D Goecking A Jorissen S de Koff C Kuss A P Schoenmakers J Vink E Waelde Astron. Astrophys. 304 415 1995 1995A&A...304..415V stars: individual (eta Car) stars: oscillations stars: variables: other supergiants techniques: photometric We present and analyze two seasons of intense photometric monitoring in the Stroemgren uvbyH{beta} system of {eta} Carinae (October 1992-August 1994). The luminous blue variable (LBV) in the core did not show much S Dor activity, i.e. it was in a relatively quiescent stage. This situation was very favourable for studying its optical micro variations. It appears that the central LBV pulsates (presumably in a non-radial mode) like other massive evolved stars, the {alpha} Cyg variables. The quasi-period is 58.56d. The linear ephemeris is: JD_max_=2448875.0 +58.56 E. Support was found for the existence of the presumed periodicity of 52.4d of the so-called "dimples", shallow dips in the light curve which only last for a few days. The cause may be the eclipse of a small companion or of a hot spot in an accretion disk. The H{beta} index became bluer by ~0.07mag during the last 11/2 years and shows an oscillation in anti-phase with the 58.56d pulsation, suggesting that the HII region(s) responsible for the hydrogen line emission has a relatively high luminosity. This is another reason to suppose that a second luminous source, perhaps a luminous disk (with a hot spot), may be present in the {eta} Car system.
eta Car HR 4210 HD 93308 10 45 03.6 -59 41 03
Stroemgren uvbyH-beta photometry of Eta Car JD Julian date d u_JD Uncertainty flag on JD --- ymag y Stroemgren magnitude mag bmag b Stroemgren magnitude mag vmag v Stroemgren magnitude mag umag u Stroemgren magnitude mag Hbmag H{beta} Stroemgren magnitude mag Simona Mei CDS 1995 Jul 26 J_A+A_304_415.xml Properties of Cool Flares with GOES class B5 to C2 J/A+A/304/563 J/A+A/304/563 Cool X-ray flares of Sun with GOES Properties of Cool Flares with GOES class B5 to C2 K J H Phillips U Feldman Astron. Astrophys. 304 563 1995 1995A&A...304..563P Sun: flares Sun: X-rays, gamma rays Observed parameters for 208 small flares with GOES classification B5 to C2 are discussed using data from the broad-band detectors on the Geostationary Operational Environmental Satellites (GOES) and the Bragg Crystal Spectrometer (BCS) on the Yohkoh solar flare spacecraft. Peak temperatures derived from He-like sulfur spectra are in the range 8+/-2x10^6^K and are similar to those derived from the ratio of the 1-8A and 0.5-4A GOES channels, but a little less than those from He-like calcium spectra, showing that even these small flares are non-isothermal. The absence of He-like iron emission shows that the temperatures are less than 14x10^6^K. There is a slight positive correlation between temperature and emission measure from the calcium and sulfur data. Differences in this distribution and that derived for larger flares in a separate study can be reconciled in terms of the fact that temperatures were measured from He-like iron spectra for the larger flares. The emission measure of the flares in our sample are correlated with GOES class. A detailed study of a subset of 20 flares shows that the temperatures generally reach peak flux slightly before (up to 30s) or coincident with the light curve maximum. It is found that even small flux enhancements which are frequently present are associated with temperature enhancements.
Properties of cool flares observed by Yohkoh Date Date of each event "YY/MM/DD" UTh Universal Time for each event h UTm Universal Time for each event min UTs Universal Time for each event s Flux(Ca) Peak flux of photons in the He-like Ca resonance (w) line ct/cm2/s Flux(S) Peak flux of photons in the He-like S resonance (w) line ct/cm2/s Te(Ca) Temperature deduced from the Ca X-ray spectrum MK Te(S) Temperature deduced from the S X-ray spectrum MK Ne2V(Ca) Emission measure for Ca cm-3 Ne2V(S) Emission measure for S cm-3 MaxFlux X-ray emission at peak as determined from GOES detectors number=1 In the 1-8 Angstroem band W/m2 Preflare X-ray emission before the flare as determined from GOES detectors number=1 In the 1-8 Angstroem band W/m2 Te(GOES) Temperatures measure from the ratio of GOES detectors MK Ne2V(GOES) Emission measure from the ratio of GOES detectors cm-3 n_Ne2V(GOES) When 'c': event selected for detailed study --- Simona Mei CDS 1995 Jun 29 J_A+A_304_563.xml Empirical study of departures from the excitation equilibrium of Fe I in metal-poor stars J/A+A/305/245 J/A+A/305/245 Fe I in metal-poor stars Empirical study of departures from the excitation equilibrium of Fe I in metal-poor stars P Magain G Zhao Astron. Astrophys. 305 245 1996 1996A&A...305..245M Abundances Equivalent widths Galaxy: abundances stars: abundances stars: Population II A detailed analysis of neutral iron lines in a sample of 13 metal-poor dwarfs and subgiants is carried out on the basis of high resolution spectra obtained with the ESO Coude Echelle Spectrometer. The deduced iron abundance is found to depend on the excitation potential of the line used, higher excitation lines generally indicating higher abundances. This could be caused by departures from the local thermodynamic equilibrium (LTE) or by temperature inhomogeneities in the stellar atmospheres. The dependency of this effect on the stellar atmospheric parameters is investigated. From the comparison of iron lines with lines of other elements, it is concluded that the low excitation Fe I lines are much more affected than the high excitation lines. The consequences of these effects for the classical abundance analyses are examined. It is found that they may explain, at least in part, some previously reported discrepancies between the results of different authors.
HD 3567 00 38 31.8 -08 18 07 HD 25704 04 01 42.6 -57 12 45 HD 122196 14 01 03.9 -38 02 59 HD 126793 14 30 12.7 -62 51 41 HD 132475 14 59 51.6 -22 00 20 HD 152924 17 00 46.7 -64 33 01 HD 160617 17 42 49.5 -40 18 55 HD 166913 18 16 27.3 -59 24 04 HD 189558 20 01 01.2 -12 15 02 HD 193901 20 23 33.8 -21 21 22 HD 194598 20 26 11.4 +09 27 28 HD 196892 20 40 49.1 -18 47 13 HD 199289 20 58 07.7 -48 12 01
Equivalent widths and abundances Element Element --- Lambda Line wavelength 0.1nm EW3567 Equivalent width for the star HD 3567 0.1pm Ab3567 Abundance for the star HD 3567 number=1 Abundance = log[Element/H]+12 --- EW25704 Equivalent width for the star HD 25704 0.1pm Ab25704 Abundance for the star HD 25704 number=1 Abundance = log[Element/H]+12 --- EW122196 Equivalent width for the star HD 122196 0.1pm Ab122196 Abundance for the star HD 122196 number=1 Abundance = log[Element/H]+12 --- EW126793 Equivalent width for the star HD 126793 0.1pm Ab126793 Abundance for the star HD 126793 number=1 Abundance = log[Element/H]+12 --- EW132475 Equivalent width for the star HD 132475 0.1pm Ab132475 Abundance for the star HD 132475 number=1 Abundance = log[Element/H]+12 --- EW152924 Equivalent width for the star HD 152924 0.1pm Ab152924 Abundance for the star HD 152924 number=1 Abundance = log[Element/H]+12 --- EW160617 Equivalent width for the star HD 160617 0.1pm Ab160617 Abundance for the star HD 160617 number=1 Abundance = log[Element/H]+12 --- EW166913 Equivalent width for the star HD 166913 0.1pm Ab166913 Abundance for the star HD 166913 number=1 Abundance = log[Element/H]+12 --- EW189558 Equivalent width for the star HD 189558 0.1pm Ab189558 Abundance for the star HD 189558 number=1 Abundance = log[Element/H]+12 --- EW193901 Equivalent width for the star HD 193901 0.1pm Ab193901 Abundance for the star HD 193901 number=1 Abundance = log[Element/H]+12 --- EW194598 Equivalent width for the star HD 194598 0.1pm Ab194598 Abundance for the star HD 194598 number=1 Abundance = log[Element/H]+12 --- EW196892 Equivalent width for the star HD 196892 0.1pm Ab196892 Abundance for the star HD 196892 number=1 Abundance = log[Element/H]+12 --- EW199289 Equivalent width for the star HD 199289 0.1pm Ab199289 Abundance for the star HD 199289 number=1 Abundance = log[Element/H]+12 --- table4.tex LaTeX version of table4 Simona Mei CDS 1995 Jun 07 J_A+A_305_245.xml The chemical composition of the s-Cepheids. II J/A+A/305/551 J/A+A/305/551 Chemical composition of the s-Cepheids The chemical composition of the s-Cepheids. II S M Andrievsky V V Kovtyukh I A Usenko Astron. Astrophys. 305 551 1996 1996A&A...305..551A Abundances Stars, variable Cepheids stars: abundances stars: evolution On the base of photographic, Reticon and CCD spectra analysis we have derived the abundances for 8 s-Cepheids and V1162 Aql (before classified as s-Cepheid). The following results have been obtained: 1) all Cepheids (excluding only EU Tau) have solar-like abundances of {alpha}- and iron-group elements, 2) Na is over abundant for all program stars, 3) the carbon deficiency found for EU Tau, DT Cyg, V440 Per and nitrogen overabundance (DT Cyg), show that these s-Cepheids are not crossing the instability strip for first time, 4) s-process elements are slightly enhanced in the program stars, 5) V1162 Aql does not show any changes in C and N abundances. The most plausible explanation is that this star is a normal Cepheid (C{delta}), but it is firstly crossing the instability strip toward the giant branch. This conclusion is also confirmed by its position on the evolutionary diagram.
V440 Per HD 14662 02 23 51.7 +55 21 53 SU Cas HD 17463 02 51 58.7 +68 53 19 SZ Tau HD 29260 04 37 14.7 +18 32 35 EU Tau HD 38321 05 45 40.5 +18 39 25 Y Oph HD 162714 17 52 38.6 -06 08 37 FF Aql HD 176155 18 58 14.6 +17 21 40 DT Cyg HD 201078 21 06 30.1 +31 11 05 V1334 Cyg HD 203156 21 19 22.1 +38 14 15
Abundances for SU Cas. Element Element --- [X/H]1 Abundance of the element for phase=0.477 Sun e_[X/H]1 Error on abundance Sun o_[X/H]1 Number of observations --- [X/H]2 Abundance of the element for phase=0.627 Sun e_[X/H]2 Error on abundance Sun o_[X/H]2 Number of observations --- [X/H]LL81 Abundance of the element from Luck and Lambert 1981 Sun Abundances for EU Tau. Element Element --- [X/H]1 Abundance of the element for phase=0.297 Sun e_[X/H]1 Error on abundance Sun o_[X/H]1 Number of observations --- [X/H]2 Abundance of the element for phase=0.323 Sun e_[X/H]2 Error on abundance Sun o_[X/H]2 Number of observations --- [X/H]3 Abundance of the element for phase=0.758 Sun e_[X/H]3 Error on abundance Sun o_[X/H]3 Number of observations --- Abundances for DT Cyg. Element Element --- [X/H]1 Abundance of the element for phase=0.155 Sun e_[X/H]1 Error on abundance Sun o_[X/H]1 Number of observations --- [X/H]2 Abundance of the element for phase=0.774 Sun e_[X/H]2 Error on abundance Sun o_[X/H]2 Number of observations --- [X/H]3 Abundance of the element for phase=0.814 Sun e_[X/H]3 Error on abundance Sun o_[X/H]3 Number of observations --- [X/H]LL81 Abundance of the element from Luck and Lambert 1981 Sun Abundances for SZ Tau. Element Element --- [X/H]1 Abundance of the element for phase=0.119 Sun e_[X/H]1 Error on abundance Sun o_[X/H]1 Number of observations --- [X/H]2 Abundance of the element for phase=0.501 Sun e_[X/H]2 Error on abundance Sun o_[X/H]2 Number of observations --- Abundances for V 1334 Cyg. Abundances for V1162 Aql. Abundances for Y Oph. Element Element --- [X/H] Abundance of the element Sun e_[X/H] Error on abundance Sun o_[X/H] Number of observations --- Abundances for FF Aql. Element Element --- [X/H]1 Abundance of the element for phase=0.780 Sun e_[X/H]1 Error on abundance Sun o_[X/H]1 Number of observations --- [X/H]2 Abundance of the element for phase=0.864 Sun e_[X/H]2 Error on abundance Sun o_[X/H]2 Number of observations --- Abundances for V440 Per. Element Element --- [X/H]1 Abundance of the element for phase=0.080 Sun e_[X/H]1 Error on abundance Sun o_[X/H]1 Number of observations --- [X/H]2 Abundance of the element for phase=0.218 Sun e_[X/H]2 Error on abundance Sun o_[X/H]2 Number of observations --- [X/H]3 Abundance of the element for phase=0.374 Sun e_[X/H]3 Error on abundance Sun o_[X/H]3 Number of observations --- [X/H]4 Abundance of the element for phase=0.385 Sun e_[X/H]4 Error on abundance Sun o_[X/H]4 Number of observations --- [X/H]L82 Abundance of the element from Luck 1982 Sun tables.tex LaTeX version of tables Simona Mei CDS 1995 Jun 07 J_A+A_305_551.xml ROSAT observations of three edge-on spiral galaxies J/A+A/305/74 J/A+A/305/74 NGC 4565, 4656 & 5907 ROSAT observations ROSAT observations of three edge-on spiral galaxies A Vogler W Pietsch P T Kahabka Astron. Astrophys. 305 74 1996 1996A&A...305...74V IX/11 : ROSAT Source Catalog (Voges+ 1994) Galaxies, optical X-ray sources galaxies: individual (NGC 4565, NGC 4656, NGC 5907) galaxies: spiral X-rays: galaxies The edge-on spiral galaxies NGC 4565, NGC 4656, and NGC 5907 have been observed with the PSPC onboard ROSAT. The targets were selected for low galactic foreground absorption to enable the detection of "soft" X-ray emission, which is a fingerprint for the emission of a million degree gaseous component. For NGC 4565 we find an X-ray luminosity of 1.1x10^40^erg/s . Point sources contribute 6.0x10^39^erg/s in the bulge and 0.7x10^39^erg/s in the disk. 1.2x10^39^erg/s may be due to diffuse X-ray emission in the bulge or disk. A nuclear source (L_x_=2.7x10^39^erg/s) is visible. In the halo of NGC 4565 diffuse emission with a luminosity of 2.6x10^39^erg/s was detected. The X-ray data indicate low absorption and soft spectra. Attributing the entire diffuse flux to emission of a hot thermal plasma, its density, mass, and cooling time are n=0.6x10^-3cm^-3/sqrt({eta}), m=2.2x10^7^Ms_{sun}_.sqrt({eta}) and {tau}=4.2x10^8^y.sqrt({eta}), respectively (with the filling factor {eta}). The disturbed galaxy NGC 4656 shows a luminosity of 1.5x10^39^erg/s, composed of a weak nuclear point source (L_x_=1.3x10^38^erg/s), five further point sources in the disk (L_x_=1.0x10^39^erg/s), and remaining diffuse emission components (L_x_=0.3x10^39^erg/s). No diffuse emission could be established in the halo of NGC 4656. NGC 5907 has an overall X-ray luminosity of 6.5x10^39^erg/s. The only point source in the bulge coincides with the nucleus (L_x_=2.8x10^39^erg/s), three point sources in the disk show an integral luminosity of 3.2x10^39^erg/s. Neither X-ray emission from SN 1940a in NGC 5907 nor diffuse halo emission could be found. The different X-ray components for the three galaxies are discussed and compared to results from other wavelength regimes.
ROSAT NGC 4565 12 36.3 +25 58 NGC 4656 12 44.2 +32 12 NGC 5907 15 15.9 +56 19
Sources in bulge, disk, and halo of NGC 4565 Sources in bulge, disk, and halo of NGC 4656 Sources in bulge, disk, and halo of NGC 5907 Serendipitous detections of sources in field A Serendipitous detections of sources in field B Serendipitous detection of sources in field C Field Field designation --- Name Source name --- RAh Rights ascension (2000) h RAm Rights ascension (2000) min RAs Rights ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec e_Pos rms uncertainty on position arcsec L(Exist) Likelihood of existence ---- Counts Net counts in the ROSAT 0.1-2.4keV band ct e_Counts rms uncertainty on Counts number=1 In table 17, in the printed version, Counts for A43 is 29.8 +/- -9.2. In electronic table17, we transform e_Counts=-9.2 to 9.2 ct HR1 Hard ratio 1 --- HR2 Hard ratio 2 --- Rate Count rate for the 0.1-2.4keV band 10-3ct/s e_Rate rms uncertainty on Rate 10-3ct/s FWHMExt FWHM of the extent number=2 FWHM and likelihood of extent for sources for which the extent exceeds the PSPC PRF and for which the likelihood of extent is >=9. arcsec lExt Likelihood of extent number=2 FWHM and likelihood of extent for sources for which the extent exceeds the PSPC PRF and for which the likelihood of extent is >=9. --- Proposed identifications of serendipitous detections in field A, B. and C Source Source name --- Candidate Candidate --- Err Distance of X-ray detection number=1 Distance of X-ray detection and proposed identification in arcsec, including a 4" systematical error of the X-ray position, no error quoted for extended objects. arcsec Err2 Second value of Err (for A27 only) arcsec Ref References number=2 References: PI,PII first and second PALOMAR survey GC Gregory & Condon (1991ApJS...75.1011G) GSC guide star catalogue from EXOSAT database, Astrophysics Division at ESTEC SIM SIMBAD catalogue, MPE database HB Hewett & Burbridge (1989, A new Catalog of Quasi-Stellar Objects, stored on magnetic tape 1989) MB Mazarella & Balzano (1986ApJS...62..751M) --- James Marcout, Patricia Bauer CDS 1997 Apr 11 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+A_305_74.xml Interstellar sulfur isotopes and stellar oxygen burning J/A+A/305/960 J/A+A/305/960 Interstellar S isotopes Interstellar sulfur isotopes and stellar oxygen burning Y -N Chin C Henkel J B Whiteoak N Langer E B Churchwell Astron. Astrophys. 305 960 1996 1996A&A...305..960C Radio lines Galaxy: abundances Galaxy: evolution ISM: abundances ISM: molecules nuclear reactions, nucleosynthesis, abundances radio lines: ISM A ^12^C^32^S, ^13^C^32^S, ^12^C^34^S, and ^12^C^33^S J=2-1 line survey has been made to study interstellar ^32^S/^34^S and ^34^S/^33^S ratios from the galactic disk. The four CS isotopomers were detected in 20 star forming regions with galactocentric distances between 3 and 9kpc. From a comparison of line velocities, the C^33^S J=2-1 rest frequency is ~250kHz below the value given in the Lovas (1992) catalog. Taking ^12^C/^13^C ratios from Wilson & Rood (1994) and assuming equal ^12^C^32^S and ^13^C^32^S excitation temperatures and beam filling factors, ^12^C^32^S opacities are in the range 3 to 15; average ^32^S/^34^S and ^34^S/^33^S isotope ratios are 24.4+/-5.0 and 6.27+/-1.01, respectively. While no systematic variation in the ^34^S/^33^S isotope ratio is found, the ^32^S/^34^S ratio increases with galactocentric distance when accounting for the ^12^C/^13^C gradient of the galactic disk. A fit to the unweighted data yields ^32^S/^34^S=3.3+/-0.5(D_GC_/kpc)+4.1+/-3.1 with a correlation coefficient of 0.84. Since the interstellar sulfur (S) isotopes are synthesized by oxygen burning in massive stars, consequences for nucleosynthesis and models of chemical evolution are briefly discussed.
Line parameters from unsmoothed J=2-1 spectra of the four measured CS isotopomers Object Object --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin Des Declination (1950) arcsec Molec Molecule --- rms rms noise of the spectrum in units of Tmb number=1 rms contains the r.m.s. noise of the spectrum in units of Tmb. This is only then equivalent to the Tmb r.m.s. error, if the line is only seen in one channel. If the line is broader, the error in Tmb is smaller. mK IntTmb Integral of main beam brightness temperature in the velocity K.km/s e_IntTmb Error on the integral of main beam brightness temperature in the velocity K.km/s Tmb Main beam brightness temperature K VLSR LSR velocity km/s FWHM Full width to half maximum linewidths km/s Vel1 Lower value of the velocity range km/s Vel2 Upper value of the velocity range km/s Simona Mei CDS 1995 Sep 07 J_A+A_305_960.xml NTT V, I and Gunn z colour-magnitude diagrams of Liller 1: a globular cluster as metal-rich as the inner bulge stellar population ? J/A+A/306/134 J/A+A/306/134 Liller 1 NTT V, I and Gunn z colour-magnitude diagrams of Liller 1: a globular cluster as metal-rich as the inner bulge stellar population ? S Ortolani E Bica B Barbuy Astron. Astrophys. 306 134 1996 1996A&A...306..134O globular clusters: individual (Liller 1) Hertzsprung-Russell (HR diagram) stars: abundances We carried out VRI and Gunn z observations of the obscured globular cluster Liller 1. The cluster is so reddened (A_V_=~9.0) that it is at the detection limit in V. The RGB in I vs. (I-z) shows a strong curvature. Recalling that the nearly solar metallicity globular clusters NGC 6553 and NGC 6528 present similar blanketing effects only in the visible bandpasses, we conclude that Liller 1 is considerably more metal-rich than these clusters. The CMD comparison of Liller 1 with the inner bulge field around it (located =~5deg from the nucleus), suggests that the cluster is as metallic as the most metallic fraction of this inner bulge population. Similarly deep I and z observations at =~0.5deg away from Liller 1, at the nominal position of Grindlay 1 do not reveal any cluster.
Cl Liller 1 C 1730-333 17 33 24.0 -33 23 16
I, Gunn z photometry of Liller1 Number Sequence number --- Xpos X pixel coordinate pix Ypos Y pixel coordinate pix Imag I magnitudes mag Gmag Gunn z instrumental magnitudes mag RDist Radial distance to cluster center pix Simona Mei CDS 1995 Jul 05 Barbuy B. <BARBUY@mesioa.obspm.fr> J_A+A_306_134.xml Spectrophotometric observations of planetary nebulae high above the Galactic plane J/A+A/307/215 J/A+A/307/215 Spectrophotomety of planetary nebulae Spectrophotometric observations of planetary nebulae high above the Galactic plane F Cuisinier A Acker J Koeppen Astron. Astrophys. 307 215 1996 1996A&A...307..215C V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) Planetary nebulae Galaxy: abundances ISM: abundances planetary nebulae: general Spectrohotometric observations at high signal-to-noise ratio for a sample of 62 planetary nebulae are presented, together with the plasma and abundance analyses. The objects were selected homogeneously from the `Strasbourg-ESO Catalogue of Galactic Planetary Nebulae' by their height above the disk (over 300pc) and their H{beta} surface brightness (between 10^-12^ and 10^-14^mW/m^2^/arcsec^2^). The abundances of O, S, Ar, and Cl are tighly correlated. The N/O ratio shows a wide range of values, independent of He or O abundance.
Measured line intensities, normalized to I(H{beta})=100. Name PNG name (see in catalogue <V/84>) --- Ident Other name --- Qual Accuracy of the line intensity number=1 For each nebula, the quality class (A, B, C) indicates the accuracy of the line intensities (see Table 1 in the paper) --- 4102 Intensity at 4102A; H I --- 4340 Intensity at 4340A; H I --- 4363 Intensity at 4363A; [O III] --- 4388 Intensity at 4388A; He I --- 4472 Intensity at 4472A; He I --- n_4472 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 4542 Intensity at 4542A; He II --- n_4542 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 4686 Intensity at 4686A; He II --- n_4686 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 4740 Intensity at 4740A; [Ar IV] --- 4861 Intensity at 4861A; H I --- 4922 Intensity at 4922A; He I --- n_4959 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 4959 Intensity at 4959A; [O III] --- n_5007 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 5007 Intensity at 5007A; [O III] --- 5199 Intensity at 5199A; [N I] --- 5412 Intensity at 5412A; He II --- n_5412 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 5518 Intensity at 5518A; [Cl III] --- n_5518 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 5538 Intensity at 5518A; [Cl III] --- n_5538 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 5754 Intensity at 5754A; [N II] --- 5876 Intensity at 5876A; He I --- 6300 Intensity at 6300A; [O I] --- 6312 Intensity at 6312A; [S III] --- 6364 Intensity at 6364A; [O I] --- 6435 Intensity at 6435A; [Ar V] --- 6548 Intensity at 6548A; [N II] --- n_6548 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 6563 Intensity at 6563A; H I --- n_6563 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 6584 Intensity at 6584A; [N II] --- n_6584 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 6678 Intensity at 6678A; He I --- 6716 Intensity at 6716A; [S II] --- n_6716 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 6731 Intensity at 6731A; [S II] --- n_6731 See Note number=2 S: Saturated lines E: Intensities were taken from the Strasbourg-ESO survey spectra (catalogue <V/84>) I: Intensities were estimated from short exposure spectra taken immediately afterwards p: indicates lines that are present in the spectra, but too weak to be measured --- 7006 Intensity at 7006A; [Ar V] --- 7065 Intensity at 7065A; He I --- 7136 Intensity at 7136A; [Ar III] --- 7325 Intensity at 7325A; [O II] --- Simona Mei CDS 1995 Sep 07 J_A+A_307_215.xml Redshift dependence of soft X-ray quasar spectra J/A+A/307/33 J/A+A/307/33 X-ray quasar spectra Redshift dependence of soft X-ray quasar spectra N Schartel R Walter H H Fink J Truemper Astron. Astrophys. 307 33 1996 1996A&A...307...33S IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) QSOs X-ray sources quasars: general X-rays: galaxies The analysis of the X-ray spectra of a sample of 102 X-ray bright quasars observed with ROSAT during the all-sky survey confirmed for the soft (0.1-2.4)keV energy range that the power law photon indices of radio-loud and radio-quiet quasars differ significantly from each other: <{GAMMA}>_rl_=2.23+/-0.07; <{GAMMA}>_rq_=2.54+/-0.04. These mean indices are found to be significantly steeper than those determined for the harder (0.3-3.5)keV energy band of the Einstein Observatory/IPC and the medium energy (2-10...20)keV bands of the EXOSAT/ME and Ginga/LAC experiments for identical subsets of quasars. The comparison yielded a tendency of the harder the energy range covered by the experiment the flatter the average spectral indices.
ROSAT
The sample, ordered by redshift and grouped to redshift bins No Sequential number --- Type q: Radio-quiet quasar l: radio-loud quasar --- QSO Quasar name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec z Redshift --- Vmag V magnitude mag MVmag Absolute V magnitude mag log(nuLnu) Optical luminosity number=1 The optical luminosity was calculated using the calibration log({nu}L_{nu})=-0.4M_V_ + 35.357 +0.4F_{nu}_E(B-V) for {nu}=5.45x10^14^Hz or lambda=5500A 10-7W alphaRO Radio to optical fluxes ratio --- Spectral characteristics No Sequential number --- Type q: radio-quiet quasar, l: radio-loud quasar --- QSO Quasar name --- Exp Exposure s Count Count rate ct/s e_Count rms uncertainty on Count ct/s HR1 Hardness ratio 1 number=1 HR1=(B-A)/(A+B) and HR2=(D-C)/(D+C) where A = count rate in PHA range 11-41 (~0.1-0.4keV) B = count rate in PHA range 52-201 (~0.5-2.0keV) C = count rate in PHA range 52-90 (~0.5-0.9keV) D = count rate in PHA range 91-201 (~0.9-2.0keV) (PHA = Pulse Height Amplitude) --- e_HR1 rms uncertainty on HR1 --- HR2 Hardness ratio 2 number=1 HR1=(B-A)/(A+B) and HR2=(D-C)/(D+C) where A = count rate in PHA range 11-41 (~0.1-0.4keV) B = count rate in PHA range 52-201 (~0.5-2.0keV) C = count rate in PHA range 52-90 (~0.5-0.9keV) D = count rate in PHA range 91-201 (~0.9-2.0keV) (PHA = Pulse Height Amplitude) --- e_HR2 rms uncertainty on HR2 --- b b parameter number=1 HR1=(B-A)/(A+B) and HR2=(D-C)/(D+C) where A = count rate in PHA range 11-41 (~0.1-0.4keV) B = count rate in PHA range 52-201 (~0.5-2.0keV) C = count rate in PHA range 52-90 (~0.5-0.9keV) D = count rate in PHA range 91-201 (~0.9-2.0keV) (PHA = Pulse Height Amplitude) --- c c parameter number=1 HR1=(B-A)/(A+B) and HR2=(D-C)/(D+C) where A = count rate in PHA range 11-41 (~0.1-0.4keV) B = count rate in PHA range 52-201 (~0.5-2.0keV) C = count rate in PHA range 52-90 (~0.5-0.9keV) D = count rate in PHA range 91-201 (~0.9-2.0keV) (PHA = Pulse Height Amplitude) --- Best fit parameters No Sequence number --- Type q: radio-quiet quasar l: radio-loud quasar --- QSO Quasar name --- N(H) Hydrogen column density 10+20cm-2 E_N(H) Error in N(H) (upper limit) 10+20cm-2 e_N(H) Error in N(H) (lower limit) 10+20cm-2 Gamma Photon index --- E_Gamma Error in Gamma (upper limit) --- e_Gamma Error in Gamma (lower limit) --- N(H)Gal Galactic hydrogen column density 10+20cm-2 n_N(H)Gal a: from Elvis et al. (1989) --- GammaGal Galactic photon index --- E_GammaGal Error in GammaGal (upper limit) --- e_GammaGal Error in GammaGal (lower limit) --- F1-24 ROSAT band (0.1-2.4)keV flux 10-11mW/m2 e_F1-24 rms uncertainty on F1-24 10-11mW/m2 log(nuFnu) Spectral flux density at 2 keV 10-11mW/m2 e_log(nuFnu) rms uncertainty on nuFnu 10-11mW/m2 log(nuLnu) Luminosity at 2 keV 10-7W Patricia Bauer CDS 1996 Sep 11 Roland WALTER <Roland.Walter@obs.unige.ch> J_A+A_307_33.xml Red giants in open clusters: V. NGC 2099 J/A+A/307/80 J/A+A/307/80 Velocities of red giants in NGC 2099 Red giants in open clusters: V. NGC 2099 J -C Mermilliod G Huestamendia G Del Rio M Mayor Astron. Astrophys. 307 80 1996 1996A&A...307...80M Clusters, open Radial velocities binaries: spectroscopic open clusters and associations: individual (NGC 2099) techniques: radial velocities 474 radial-velocity observations and new UBV photoelectric data for 55 and 20 red giants respectively, in the field of the intermediate-age open cluster NGC 2099 are presented and analysed for membership and duplicity. The membership of 35 red giants has been confirmed, 16 spectroscopic binaries have been discovered and 11 orbits have been determined. The cluster binary-frequency lower limit is slightly above the average (9/35=26%). The radial distribution of the red giants shows a sharp limit between members and non-members. No mass segregation is observed between the binary and single red giants. The latest isochrones from the Geneva and Padova groups reproduce very well the observed morphology in the colour-magnitude diagram for log t=8.65 and z=0.02, with (m-M)=11.50 and E(B-V)=0.29. Other papers in the series: Paper I =1989A&A...219..125M : NGC 2447, 2539, 2632, 6633 and 6940 Paper II =1989A&AS...79...11M : Binaries in NGC 2360, 2437, 2447, 5822, 5823 and 6475 Paper III =1990A&A...237...61M : NGC 2360, 2423, 5822, 6811 and IC 4756 Paper IV =1995A&A...299...53M : NGC 3680 and IC 4651 Paper VI =1997A&A...319..481M : Binaries in NGC 2489, 2567, 3033, 5822, 6134, 6664 and IC 2488
NGC 2099 M37 05 52.3 +32 33
Radial velocity data for NGC 2099 ID Star number number=1 The numbering system used for NGC 2099 is from: von Zeipel H., Lindgren J. 1921, Kungl.Sven.Vet.Handl. 61 no 15 (1921KSVH...61...15V) --- HJD Heliocentric Julian Date d Comp Component of a double-lined binary --- RV Radial velocity km/s e_RV Error on the radial velocity km/s Simona Mei CDS 1995 Aug 17 Jean-Claude Mermilliod <mermio@scsun.unige.ch> J_A+A_307_80.xml Observation of the metallic line doubling phenomenon in the variable star RR Lyrae. J/A+A/308/481 J/A+A/308/481 Metallic line doubling phenomenon in RR Lyrae Observation of the metallic line doubling phenomenon in the variable star RR Lyrae. M Chadid D Gillet Astron. Astrophys. 308 481 1996 1996A&A...308..481C Line Profiles Stars, variable hydrodynamics shock waves stars: individual (RR Lyrae) stars: pulsation For the first time, the observation of the line doubling phenomenon over two metallic absorption lines of a RR Lyrae star (RR Lyr) is reported. A resolving power of 42,000 and a time resolution close to 1% of the pulsating period were necessary. Although a smaller exposure time would be required to completely resolve this phenomenon over the whole spectrum, we interpret it as the consequence of a "two-step" Schwarzschild's mechanism. Thus a strong shock wave propagating throughout the photosphere around phase 0.93 would be at the origin of the observed line doubling. Because the shock undergoes a sudden acceleration phase, a "jump" appears in the line profile evolution. The shock is first receding and then almost stationary. Our qualitative interpretation needs a theoretical confirmation with the help of a nonlinear nonadiabatic pulsational model with an extended atmosphere taking into account the presence of shock waves. Nevertheless it appears from our observations that the dynamics of the atmosphere of RR Lyr is important just above the photosphere and that strong shock exists at this level because the doubling is already present in FeI lines.
RR Lyr HD 182989 19 25 28.3 +42 47 14
*Journal of the spectrovelocimetric observations of RR Lyr Phi Phase number=1 According to the ephemeris: HJD (maximum brightness) = 2444003.8537 + 0.566839*E. --- JD Julian Date d Time Exposure time s S/N Signal to noise ratio --- HRV Heliocentric radial velocity km/s Sigma FWHM/2.35 of the line km/s Amp Line deep --- Simona Mei CDS 1995 Sep 18 J_A+A_308_481.xml A search for precursors of ultracompact HII regions in a sample of luminous IRAS sources. I. Association with ammonia cores. J/A+A/308/573 J/A+A/308/573 Ammonia on YSOs IRAS sources A search for precursors of ultracompact HII regions in a sample of luminous IRAS sources. I. Association with ammonia cores. S Molinari J Brand R Cesaroni F Palla Astron. Astrophys. 308 573 1996 1996A&A...308..573M Radio lines YSOs circumstellar matter HII regions ISM: molecules radio lines: ISM stars: formation stars: pre-main sequence We present observations of NH_3_ (1,1) and (2,2) lines in two flux-limited samples of IRAS sources selected according to colour criteria which should result in a high fraction of Young Stellar Objects. The first sample contains sources (named 'LOW') whose evolutionary status is essentially unknown, while the second sample contains sources (named 'HIGH') possibly associated with ultracompact HII regions, the distinction being based on the IRAS [25-12] colour.
General informations about observed sources. Seq Running number --- IRAS IRAS name --- Type Source type (H --> HIGH; L --> LOW) --- n_Type A '^' means a 12um flux upper limit for that source --- RAh 1950 hours of Right Ascension h RAm 1950 minutes of Right Ascension min RAs 1950 seconds of Right Ascension s DE- sign for declination --- DEd 1950 degrees of Declination deg DEm 1950 arcmin of Declination arcmin DEs 1950 arcsec of Declination arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Dist Distance from observer kpc n_Dist Note on distance number=1 'a' means that the distance ambiguity has been resolved 'b' means the the distance of the tangent point has been assumed --- Lum Bolometric luminosity solLum NH3det Y/N flag indicating detection in ammonia --- H2Odet Y/N flag indicating detection in water maser --- IDent Other identification from the literature --- Ammonia line parameters and deduced physical quantities Seq Running number (as in Table1.dat) --- T11 Antenna temperature for line (J,K)=(1,1) K e_T11 Percentage uncertainty on T11 % V11 (1,1) center line velocity km/s e_V11 Percentage uncertainty on V11 % W11 (1,1) FWHM km/s e_W11 Percentage uncertainty on W11 % T22 Antenna temperature for line (J,K)=(2,2) K e_T22 Percentage uncertainty on T22 % V22 (2,2) center line velocity km/s e_V22 Percentage uncertainty on V22 % W22 (2,2) FWHM km/s e_W22 Percentage uncertainty on W22 % Tkin Ammonia kinetic temperature K l_Tkin flag indicating that Tkin is a limit --- e_Tkin Percentage uncertainty on Tkin % Ncol Ammonia column density cm-2 l_Ncol flag indicating that Ncol is a limit --- e_Ncol Percentage uncertainty on Ncol % l_Tau indicates if the Tau value is upper limit --- Tau Optical depth of (1,1) line --- e_Tau Percentage uncertainty on Tau % Patricia Bauer CDS 1996 Apr 16 Sergio Molinari, <smolinar@isows4.vilspa.esa.es> J_A+A_308_573.xml NTT VI photometry of the metal-rich and obscured bulge globular cluster Terzan 5. J/A+A/308/733 J/A+A/308/733 NTT VI photometry in Terzan 5 NTT VI photometry of the metal-rich and obscured bulge globular cluster Terzan 5. S Ortolani B Barbuy E Bica Astron. Astrophys. 308 733 1996 1996A&A...308..733O Clusters, globular Photometry globular clusters: general globular clusters: individual (Terzan 5) Hertzsprung-Russell (HR diagram) We study the metal-rich bulge globular cluster Terzan 5 by means of VI colour-magnitude diagrams, with images obtained under exceptional seeing conditions (0.34"-0.50"). Differential reddening is important across the cluster. We derive a reddening of E(B-V)=2.49 and a distance from the Sun d_{sun}_=5.6kpc, closer than previous estimates. Based on the red giant branch curvature, we derive a metallicity somewhat higher than that of NGC 6553, probably solar.
Terzan 5 17 48.1 -24 47
V, I photometry of Terzan 5 Number Sequence number --- Xpos X pixel coordinate pix Ypos Y pixel coordinate pix Vmag V magnitude mag V-I (V-I) colour index mag Simona Mei CDS 1995 Aug 18 J_A+A_308_733.xml ROSAT observations of ten globular clusters with large core radii J/A+A/309/116 J/A+A/309/116 10 globular cluster ROSAT observations ROSAT observations of ten globular clusters with large core radii H M Johnston F Verbunt G Hasinger Astron. Astrophys. 309 116 1996 1996A&A...309..116J Clusters, globular X-ray sources globular clusters: general X-rays: stars We present X-ray observations of ten globular clusters observed with the ROSAT PSPC. The clusters were chosen to have large core radii and to be nearby. Three clusters contain X-ray sources which are probably associated with the cluster. One is the previously discovered X-ray transient H1825-331 in NGC 6652. The other two, in NGC 6366 and NGC 6809, are new members of the class of low-luminosity sources, with luminosities in the region of 10^32^erg/s. Upper limits can be placed on the source temperatures of both sources, making them similar to sources found in other globular clusters by ROSAT.
ROSAT
Detected sources Name Source name number=1 "C" represents the upper limit to the number of counts at the cluster core, for clusters where no source was detected in the core. --- Cluster Cluster name --- RAh Right ascension J2000 (hours) h RAm Right ascension J2000 (minutes) min RAs Right ascension J2000 (seconds) s DE- Declination J2000 sign --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Delta Offset from core (core radii) --- Cts Counts number=2 Counts <0 indicate an upper limit ct e_Cts Error on counts ct S 0.5-2.5 keV X-ray flux 10-24W/m2 l_HR1 Limit flag on HR1 --- HR1 Hardness ratio 1 --- e_HR1 Error on HR1 --- l_HR2 Limit flag on HR2 --- HR2 Hardness ratio 2 --- e_HR2 Error on HR2 --- ID Optical ID number=3 A source was taken to be a counterpart when the difference in position was less than about 15 arcsec. --- Offset Offset between X-ray & optical arcsec Patricia Bauer CDS 1996 Jan 12 H.M. Johnston, <HMJ@aaoepp2.aao.gov.au> J_A+A_309_116.xml The spiral structure of M51 from Halpha and 2000A UV Images. A new tracer of density waves effects. J/A+A/309/446 J/A+A/309/446 HII Regions in M51 The spiral structure of M51 from Halpha and 2000A UV Images. A new tracer of density waves effects. H Petit C T Hua D Bersier G Courtes Astron. Astrophys. 309 446 1996 1996A&A...309..446P H II regions galaxies: individual (M 51) galaxies: ISM galaxies: spiral ultraviolet: galaxies A deeper detection of the spiral structure of the Sbc galaxy M 51 is the main goal of this paper. New UV data in the 2000A range were obtained with a high altitude balloon of the Laboratoire d'Astronomie Spatiale de Marseille and the Observatoire de Geneve, (LAS-OG). The data reveal the location of hot, evolved low-mass stars predominantly along the outside edge of, and down stream from, the spiral arms defined by the string of HII regions. Since these stars have a relatively well-defined age compared to the "mixed" population of stars seen in the arms when observed in visible light, the UV data is well-suited to derive time-scales of spiral arm components. In particular, the relation between spiral structure and star formation, which is at least partly due to the density wave shock mechanism, can be studied from the differential positions of the low-mass stars observed in the UV and the massive stars coexisting with the ionized gas. To facilitate such detailed UV-H{alpha} comparison, we have also carried out new deep integrations, photometry, and accurate mapping of the H{alpha} emission. A catalogue of 478 HII regions in M 51 has been established from the analysis of narrow band H{alpha} images taken with a combination of the Special Astronomical Observatory (SAO) Russian image tube, and the Observatoire de Marseille (OM) focal reducer f/1.5 (9m equivalent focal length) attached at the prime focus of the 6-m telescope of the SAO. The radial and tangential shifts of the main and secondary spiral structures in UV and H{alpha} are also compared with other spiral tracers. The displacements observed in these observations are compatible with a scenario in which the star formation is triggered by the density wave.
M 51 NGC 5194 Whirlpool galaxy 13 29.9 +47 12
Large catalogue of the HII regions observed in M51 Source Source number --- CCM Designation in Carranza et al. 1969 (1969A&A.....1..479C) --- Xpos X position number=1 The positions of the photometric centre of Halpha emission are centered on 13 27 46.3 +47 27 10.2 (1950)(source 212); X axis is oriented toward East and Y axis toward North arcsec Ypos Y position number=1 The positions of the photometric centre of Halpha emission are centered on 13 27 46.3 +47 27 10.2 (1950)(source 212); X axis is oriented toward East and Y axis toward North arcsec Flux H{alpha} fluxes number=2 H{alpha} fluxes are given in units of 10^-16^erg/cm2/s 10-19W/m2 eDiam Effective diameter, blank if unresolved. arcsec gDiam Geometrical diameter arcsec Simona Mei CDS 1995 Oct 13 Henri Petit, Observatoire de Marseille <hpetit@obmara.cnrs-mrs.fr> J_A+A_309_446.xml Spectroscopic orbit of the triple star 55 Ursae Majoris. J/A+A/309/521 J/A+A/309/521 55 UMa spectroscopic orbit Spectroscopic orbit of the triple star 55 Ursae Majoris. J Horn J Kubat P Harmanec P Koubsky P Hadrava V Simon S Stefl P Skoda Astron. Astrophys. 309 521 1996 1996A&A...309..521H Binaries, orbits Binaries, spectroscopic Radial velocities binaries: spectroscopic stars: fundamental parameters stars: individual (55 Uma) The first investigation of the known triple system 55 UMa (2.55d binary in a ~1870-d orbit with the third star) based on electronic spectra led to several new findings about the system: (1) Discovery of spectral lines of the tertiary and an unambiguous detection of the lines of the secondary. Spectra of both primary and tertiary are of the same strength and correspond to spectral class A0V. The secondary spectrum is about twice fainter in the visual region and belongs probably also to spectral class A. (2) First self-consistent orbital solution describing close and wide orbit and the detection of apsidal motion for the close pair. The orbital period of the close pair was improved to (2.5538380+/-0.0000046d) and basic physical elements for all three stars and the system were estimated. The orbital solution also gives the period of apsidal motion of the close pair of (450+/-60)yr and leads to a good agreement with the published speckle-interferometric orbit for the distant companion if the longitude of periastron passage is increased by 180deg.
HD 98353 55 UMa HR 4380 BD +38 2225 11 19 08 +38 11 11
Radial velocities of 55 UMa Inst Instrument number=1 AUR: Aurelier spectrograph RET: Reticon in Coude spectrograph --- HJD Heliocentric Julian date d RV1a Primary radial velocity from all lines km/s w1a Weight of the particular radial velocity RV1a --- RV1 Primary radial velocity from CaI line km/s w1 Weight of the particular radial velocity RV1 --- RV2 Secondary radial velocity from CaI line km/s w2 Weight of the particular radial velocity RV2 --- W Wavelength range A Patricia Bauer CDS 1996 Feb 08 J_A+A_309_521.xml He I lambda 10830A line as an indicator of solar chromospheric activity J/A+A/309/655 J/A+A/309/655 Solar chromospheric activity He I lambda 10830A line as an indicator of solar chromospheric activity A G Shcherbakov Z A Shcherbakova I Tuominen L Jetsu Astron. Astrophys. 309 655 1996 1996A&A...309..655S Sun Sun: activity Sun: chromosphere Full disk spectroscopic observations in the near infrared region of the solar spectrum (the Sun-as-a-star) are presented for the years 1981-1993. The central depth of the He I {lambda}10830A line shows changes following the 11-year activity cycle, and also variability following the rotation of the Sun. We found high correlations between the depth of the He I line and coronal indices of activity, such as Fe XIV {lambda}5303 coronal emission index and 10.7cm radio flux. Thus the He I line depth may be used as an index of activity for the chromospheric and low chromospheric-coronal transition region for the Sun, observed as a star and, by inference for other late-type stars.
Activity indices for the Sun as a star Date Date of observations "DD/MM/YY" JD Julian Date d RHeI Line depth of local continuum (He I 10830A) % CI Coronal Index number=1 Coronal index as in Rybansky et al. 1988, 1990; Rybansky 1995; see page 2 in the paper 10+16W/sr Nspot Sunspot number --- Flux Radio Flux at 10.7 cm (in 10-22W/m2Hz) 10kJy SMF Solar Magnetic Field (in {micro}T=10-2Gauss) uT Simona Mei CDS 1995 Sep 07 J_A+A_309_655.xml The fundamental plane of early-type galaxies: stellar populations and mass-to-light ratio J/A+A/309/749 J/A+A/309/749 Fundamental plane of early type galaxies The fundamental plane of early-type galaxies: stellar populations and mass-to-light ratio P Prugniel F Simien Astron. Astrophys. 309 749 1996 1996A&A...309..749P Galaxies, optical galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: kinematics and dynamics galaxies: photometry We analyse the residuals to the fundamental plane (FP) of elliptical galaxies as a function of stellar-population indicators; these are based on the line-strength parameter Mg2 and on UBVRI broad-band colors, and are partly derived from new observations. The effect of the stellar populations accounts for approximately half the observed variation of the mass-to-light ratio responsible for the FP tilt. The residual tilt can be explained by the contribution of two additional effects: the dependence of the rotational support, and possibly that of the spatial structure, on the luminosity. We conclude to a constancy of the dynamical-to-stellar mass ratio. This probably extends to globular clusters as well, but the dominant factor would be here the luminosity dependence of the structure rather than that of the stellar population. This result also implies a constancy of the fraction of dark matter over all the scalelength covered by stellar systems. Our compilation of internal stellar kinematics of galaxies is appended.
Catalogue of central velocity dispersion Name Galaxy identifier number=1 The Name has been adopted by descending the hierarchy: (1) Usual name for the dwarf spheroidal galaxy and the Milky Way, (2) NGC name, (3) IC, (4) UGC or ESO, (5) PGC (Principal Galaxies Catalogue) (6) LEDA (Lyon- Meudon Extragalactic Database) internal identifier. For about 50 object left unfolted into this hierarchy we kept the designation from the original reference. When Name differed from the original designation, the latter is indicated in the field Note. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (min) min RAs Right Ascension 1950 (sec) s DE- Sign of declination --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec sigmam Adopted central velocity dispersion number=2 The velocity dispersions reported here are from absorption lines, except for Milky Way and the dwarf spheroidal galaxy: from individual stellar velocity, and for the references Hui93 (Hui, X. 1993) and Arna+94 (Arnaboldi et al., 1994): from planetary nebulae. km/s l_sigma Upper (<) or lower (>) limit --- sigma Central velocity dispersion (raw) number=3 sigmam is a mean of the re-scaled measured velocity dispersion, (sigma) weighted by the inverse of the squared mean error (e_sigma). The scaling factors are listed in tablea3 (scale). km/s e_sigma Mean error on sigma km/s Ref_a Acronym of the source reference number=4 Refers to tablea3 --- Ref_c Numerical code of the source ref number=5 Refers to tablea3 --- Reject [1 ] Rejection flag, 1=rejected --- Note Descriptive note or alternative name --- Catalogue of maximum velocity of rotation Name Galaxy identifier number=1 See tablea1 --- Axis Axis used for rotation measure number=2 Indicate the axis along which the rotation has been measured, coded as follow: MJ: Major axis MI: Minor axis PA: Pair axis, for binary galaxies --- Note Note on the galaxy --- l_Vmax Upper (<) or lower (>) limit --- Vmax Maximum velocity of Rotation km/s e_Vmax Mean error on Vmax km/s Ref_a Acronym of the source reference number=3 Refers to tablea3 --- Bibliographic references for tablea1 and tablea2 Ref_c Numerical code of the source ref number=1 References codes in the range [1-138] are present in McElroy 1995 (ApJS 100, 105); numbers in the range [201-351] are not; reference 500 gathers new unpublished measurements from Observatoire de Haute-Provence observations --- Ref_a Acronym of the source reference --- Scale Scaling factor to be applied number=2 The raw measurement of the velocity dispersion (sigma in tablea1) has to be multiplied by the scaling factor Scale to convert it in a homogeneous scale. --- Ref Full text of the reference --- Fundamental parameters for the galaxies in the sample Name Galaxy identifier number=1 See tablea1. --- SSample Sub-sample --- Dmod Distance modulus mag Bt Total apparent B magnitude number=2 Corrected for galactic absorption (Burstein & Heiles) and k. mag mue Mean B surface brightness with r_e number=3 Mean B surface brightness within the effective circular aperture. Corrected for galactic absorption (Burstein & Heiles), k and cosmologic (1+z)**4 dimming. mag U-B U-B color within r_e, corrected number=4 corrected for Galactic absorption with: E(U-B)=0.20 Ab k-corrected with: (U-B)corr=(U-B)raw+0.055*velocity[km/s]*1.e-4 mag B-V B-V color within r_e, corrected number=5 corrected for Galactic absorption with: E(B-V)=0.25 Ab k-corrected with: (B-V)corr=(B-V)raw+0.095*velocity[km/s]*1.e-4 mag V-R V-R color within r_e, corrected number=6 corrected for Galactic absorption with: E(V-R)=0.20 Ab k-corrected with: (V-R)corr=(V-R)raw+0.030*velocity[km/s]*1.e-4 mag V-I V-I color within r_e, corrected number=7 corrected for Galactic absorption with: E(V-I)=0.35 Ab k-corrected with: (V-I)corr=(V-I)raw+0.030*velocity[km/s]*1.e-4 mag Mg2 Mg2 index mag sigmam Adopted central velocity dispersion number=8 average weighted by the inverse square error of the re-scaled measurements km/s Vmax Maximum velocity of rotation, number=9 average weighted by the inverse square error of the MJ measurements km/s Rfp Residual from the Fundamental Plane --- Patricia Bauer CDS 1996 Jan 12 P. Prugniel, <prugniel@cumulus.univ-lyon1.fr> J_A+A_309_749.xml Rapid photometric and spectroscopic variability of the Be star DX Eridani J/A+A/309/787 J/A+A/309/787 DX Eri variability Rapid photometric and spectroscopic variability of the Be star DX Eridani S Stefl L A Balona Astron. Astrophys. 309 787 1996 1996A&A...309..787S Line Profiles Photometry, uvby Stars, Be Stars, variable stars: activity stars: emission-line, Be stars: individual (DX Eri) We present results of nearly simultaneous monitoring of uvby light and HeI667.81nm line-profile variations of the equatorial Be star DX Eri in November 1991. They are analysed along with numerous uvby photometry in the period 1986-1995.
DX Eri HR HR 1508 HD 30076 04 44 05.2 -08 30 13
La Silla photometric observations, November 1991 SAAO photometric observations, November 1991 La Silla photometric observations, December, 1992 - January, 1993 SAAO photometric observations, November 1994 La Silla photometric observations, December, 1994 - January, 1995 HJD Heliocentric Julian date of the mid-exposure d umag u magnitude mag vmag v magnitude mag bmag b magnitude mag ymag y magnitude mag Quantitative parameters measured in the HeI 667.81 nm line profiles HJD Heliocentric Julian date of the mid-exposure d RV Stellar radial velocity measured on the outer wings of the line km/s <v> First line moment (in the heliocentric wavelength scale) km/s <v>c First line moment (in the heliocentric wavelength scale corrected for the radial velocity) km/s FWHM Full width at half maximum km/s LD Difference of the central depth of the line with respect to the mean profile (in units of 10^-3^ x continuum) 10-3 EW Equivalent width 0.01nm tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Feb 08 J_A+A_309_787.xml X-ray properties of active galactic nuclei with optical FeII emission J/A+A/309/81 J/A+A/309/81 X-ray properties of AGN X-ray properties of active galactic nuclei with optical FeII emission T Wang W Brinkmann J Bergeron Astron. Astrophys. 309 81 1996 1996A&A...309...81W Active gal. nuclei Radio sources X-ray sources galaxies: active ultraviolet: galaxies X-rays: galaxies ROSAT spectra of 86 Active Galactic Nuclei (AGN) with a broad range of optical FeII strengths have been analyzed. The results of the spectral analysis have been combined with optical and radio data as well as with optical emission line properties collected from the literature to understand the origin of the strong FeII emission and the nature of the soft X-ray excess.
ROSAT
Optical and radio data Bname Name based on 1950 coordinates --- Name AGN name --- Type AGN type, Q = quasar, S1 = Seyfert 1 --- z Redshift --- Vmag Optical magnitude mag W(FeII) FeII line width 0.1nm W(Hbeta) Hbeta line width 0.1nm RFe Intensity ratio I(FeII)/I(Hbeta) --- S TOtal radio flux density mJy S60 Radio flux density at 60{mu} mJy l_FWHM limit flag on FWHM(Hbeta) --- FWHM Hbeta Full Widht Half Maximum km/s Resulting of fitting ROSAT PSPC spectrum Name AGN name --- NH Hydrogen column density 10+20cm-2 e_NH rms uncertainty on NH 10+20cm-2 Gx Photon index --- e_Gx rms uncertainty on Gx --- Norm Normalization of the power law photon flux at 1keV 10-4ph/s/cm+2/keV e_Norm rms uncertainty on Norm 10-4ph/s/cm+2/keV f_CHI2 Degrees of freedom of the CHI2 --- CHI2 Reduced CHI2 --- Com Comment --- ROSAT All Sky Survey (RASS) data of PG quasars Name AGN PG name --- NH Galactic hydrogen column density 10+20cm-2 Count Counts ct/s e_Count rms uncertainty on counts ct/s Gx Photon index --- F(2keV) X-ray flux at 2 keV 10-12mW/m+2/keV Complete Spearmann Rank Correlation Matrix Param Parameter name (Lo, Lx, etc ...) --- RLo Correlation coefficient with optical luminosity --- RLx Correlation coefficient with X-ray luminosity --- RLir Correlation coefficient with IR luminosity --- RAro Correlation coefficient with Aro number=1 Aox: average broad-band optical to X-ray spectral index Aix: average infrared to X-ray spectral index Aio: average infrared to broad-band optical spectral index Aro: average radio to broad-band optical spectral index --- RAox Correlation coefficient with Aox number=1 Aox: average broad-band optical to X-ray spectral index Aix: average infrared to X-ray spectral index Aio: average infrared to broad-band optical spectral index Aro: average radio to broad-band optical spectral index --- RAix Correlation coefficient with Aix number=1 Aox: average broad-band optical to X-ray spectral index Aix: average infrared to X-ray spectral index Aio: average infrared to broad-band optical spectral index Aro: average radio to broad-band optical spectral index --- RAio Correlation coefficient with Aio number=1 Aox: average broad-band optical to X-ray spectral index Aix: average infrared to X-ray spectral index Aio: average infrared to broad-band optical spectral index Aro: average radio to broad-band optical spectral index --- RFWHM Correlation coefficient with FWHM(Hbeta) --- RRFe Correlation coefficient with I(FeII)/I(Hbeta) --- RWHbeta Correlation coefficient with W(Hbeta) --- RWFeII Correlation coefficient with W(FeII) --- RGx Correlation coefficient with photon index --- l_PLo Limit flag for PLo --- PLo Null correlation probability with Lo --- l_PLx Limit flag for PLx --- PLx Null correlation probability with Lx --- l_PLir Limit flag for PLir --- PLir Null correlation probability with Lir --- PAro Null correlation probability with Aro --- l_PAox Limit flag for PAox --- PAox Null correlation probability with Aox --- l_PAix Limit flag for PAix --- PAix Null correlation probability with Aix --- l_PAio Limit flag for PAio --- PAio Null correlation probability with Aio --- l_PFWHM Limit flag for PFWHM --- PFWHM Null correlation probability with FWHM(Hbeta) --- l_PRFe Limit flag for PRFe --- PRFe Null correlation probability with RFe --- l_PWHbeta Limit flag for PWHbeta --- PWHbeta Null correlation probability with W(Hbeta) --- l_PWFeII Limit flag for PWFeII --- PWFeII Null correlation probability with W(FeII) --- l_PGx Limit flag for PGx --- PGx Null correlation probability with GAMMAx --- table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 table4.tex LaTeX version of table4 Patricia Bauer CDS 1996 Jan 08 J_A+A_309_81.xml Variability of classical T Tauri stars. Its relation to the accretion process J/A+A/310/143 J/A+A/310/143 Variability of classical T Tauri stars Variability of classical T Tauri stars. Its relation to the accretion process M Fernandez C Eiroa Astron. Astrophys. 310 143 1996 1996A&A...310..143F Photometry, UBVRI accretion, accretion disks stars: formation stars: pre-main sequence We present the analysis of a UBV(RI)c photometric monitoring program carried out from July 1988 to August 1992 on a sample of 13 classical T Tauri stars and 2 suspected classical T Tauri stars. We detected optical irregular variability with an amplitude larger than 0.1mag in the V band in 8 stars. For 5 of them most of the variability can be attributed to hot spots, for one, to cool spots and for two of them, there is no clear mechanism; nevertheless, other phenomena must explain the short term (hours - days) and long term (years) variations superimposed. For some objects an anomalous behaviour at the shorter wavelengths (U band) is detected. From the comparison between the amplitude of the optical variability due to hot spots and the equivalent width of the Halpha emission a correlation between them is suggested. Assuming that the Halpha emission is related to the accretion process, this correlation supports the idea that we are observing the hot spots where the material from the accretion disks falls onto the star. For a description of the (RI)c photometric system, see e.g. <GCPD/54>
Average values of the photometric observations Name Star name --- Date Observing run number=1 R and J denote the Romeo and Juliet photometers at the JKT telescope, respectively. --- Vmag V band mag B-V (B-V) colour index mag U-B (U-B) colour index mag V-R (V-R) colour index mag V-I (V-I) colour index mag Patricia Bauer CDS 1996 Feb 08 M. Fernandez <matilde@astroscu.unam.mx> J_A+A_310_143.xml The early-type multiple system Eta Orionis. II. Line profile variations in component Ab J/A+A/310/164 J/A+A/310/164 Line profile variations in eta Ori The early-type multiple system Eta Orionis. II. Line profile variations in component Ab K De Mey C Aerts C Waelkens H Van Winckel Astron. Astrophys. 310 164 1996 1996A&A...310..164D Binaries, eclipsing Binaries, spectroscopic Radial velocities binaries: eclipsing binaries: spectroscopic line: profiles stars: individual (eta Ori) stars: oscillations Eta Orionis (HD35411) is a multiple system which consists of at least four early B-type stars. In the present paper we focus on the double-lined spectroscopic eclipsing pair Aab, and in particular on component Ab, which is a remarkable intrinsically variable star. The presence of this variable in an eclipsing system enables us to determine accurately its mass, radius, inclination angle and rotation period.
Eta Ori HD 35411 HR 1788 05 24 28.58 -02 23 49.5
Barycentric radial velocity measurements of eta Ori Aa and Ab of the 1993 observations HJD Heliocentric Julian Date of observation d Phase Orbital phase --- RV1 Primary heliocentric average radial velocity km/s o_RV1 Number of lines included to obtain each average velocity for the primary --- RV2 Secondary heliocentric average radial velocity km/s Patricia Bauer CDS 1996 Feb 28 K. De Mey, <Katrien.DeMey@wis.kuleuven.ac.be> J_A+A_310_164.xml Rotational modulation and flares on RS Canum Venaticorum and BY Draconis stars. XIX. Simultaneous IUE, ROSAT, VLA, and visual observations of TY Pyxidis J/A+A/310/173 J/A+A/310/173 TY Pyx IUE FES observations Rotational modulation and flares on RS Canum Venaticorum and BY Draconis stars. XIX. Simultaneous IUE, ROSAT, VLA, and visual observations of TY Pyxidis J E Neff I Pagano M Rodono A Brown R C Dempsey D C Fox J L Linsky Astron. Astrophys. 310 173 1996 1996A&A...310..173N stars: activity stars: chromospheres stars: coronae stars: individual (HD 77137) stars: spots This is a 3-part table presenting a log of the IUE Fine-Error Sensor Observations of TY Pyxidis in November 1990. In order to determine accurate magnitudes from FES measurements, a focus and a reference-point offset corrections must be applied. The data presented in the paper (Figure 1) have these corrections applied and are averages of two or more measures taken close in time.
IUE HD 77137 TY Pyx 08 59 42.7 -27 48 55
Log of IUE Fine-Error Sensor (FES) Observations OBSdate Observation date "DD/MM/YY" OBSh Observation time (UT), hours h OBSm Observation time (UT), minutes min OBSs Observation time (UT), seconds s Count Counts (f/o), Fast-Track Overlap mode. --- dX Reference-point offset correction in X --- dY Reference-point offset corrections in Y --- Phase Phase. Phases are computed using the ephemeris HJD2443548.6695 + 3.198584E. --- Step Focus step --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 Mar 01 J_A+A_310_173.xml The ESO Nearby Abell Cluster Survey (ENACS). II. The distribution of velocity dispersions of rich galaxy clusters. J/A+A/310/31 J/A+A/310/31 The ESO Nearby Abell Cluster Survey. II. The ESO Nearby Abell Cluster Survey (ENACS). II. The distribution of velocity dispersions of rich galaxy clusters. A Mazure P Katgert R den Hartog A Biviano P Dubath E Escalera P Focardi D Gerbal G Giuricin B Jones O Le Fevre M Moles J Perea G Rhee Astron. Astrophys. 310 31 1996 1996A&A...310...31M J/A+A/310/8 : ENACS. Part I. Clusters, galaxy Redshifts Velocity dispersion cosmology: observations dark matter galaxies: clusters: general galaxies: distances and redshifts The ESO Nearby Abell Cluster Survey (the ENACS) has yielded 5634 redshifts for galaxies in the directions of 107 rich, Southern clusters selected from the ACO catalogue (Abell et al. 1989). By combining these data with another 1000 redshifts from the literature, of galaxies in 37 clusters, we construct a volume-limited sample of 128 R_ACO_>=1 clusters in a solid angle of 2.55sr centered on the South Galactic Pole, out to a redshift z=0.1. For a subset of 80 of these clusters we can calculate a reliable velocity dispersion, based on at least 10 (but very often between 30 and 150) redshifts.
*Statistical sample of 128 ACO clusters Main systems in the 'cone' with z>0.1 and N>=10 (with relevant secondary systems), and systems outside the 'cone' with N>=10 ACO Abell number of cluster --- n_ACO Code number=1 a = ESO Nearby Abell Cluster Survey (ENACS) data combined with literature b = literature data only (only in table 1a) c = system inside `cone' with z > 0.1 (only in table 1b) --- Ngal Number of galaxies in the system --- z Mean redshift of the system (if Nz=0, the z is photometric estimate) --- sigma Global velocity dispersion corrected for the effect of 'interlopers' km/s C(ACO) Background-corrected richness count, from ACO --- C(bck) Background correction applied by ACO to the apparent (raw) richness count --- C(3D) Inferred intrinsic (3D) richness, derived as C(3d)=f_main_*(C(ACO)+C(bck)), where f_main_ is the fraction of measured redshifts residing in the main system --- Patricia Bauer CDS 1996 Mar 01 Peter Katgert <katgert@strw.LeidenUniv.nl> J_A+A_310_31.xml Redshift periodicity in the Local Supercluster J/A+A/310/353 J/A+A/310/353 Redshift of 97 spirals Redshift periodicity in the Local Supercluster B N G Guthrie W M Napier Astron. Astrophys. 310 353 1996 1996A&A...310..353G Positional data Redshifts galaxies: distances and redshifts galaxies: spiral radio lines: galaxies Persistent claims have been made over the last ~15yr that extragalactic redshifts, when corrected for the Sun's motion around the Galactic centre, occur in multiples of ~24 or ~36km/s. A recent investigation by us of 40 spiral galaxies out to 1000km/s, with accurately measured redshifts, gave evidence of a periodicity ~37.2-37.7km/s. Here we extend our enquiry out to the edge of the Local Super cluster (~2600km/s), applying a simple and robust procedure to a total of 97 accurately determined redshifts. We find that, when corrected for related vectors close to recent estimates of the Sun's galactocentric motion, the redshifts of spirals are strongly periodic (P~37.6km/s). The formal confidence level of the result is extremely high, and the signal is seen independently with different radio telescopes. We also examine a further sample of 117 spirals observed with the 300-foot Green Bank telescope alone. The periodicity phenomenon appears strongest for the galaxies linked by group membership, but phase coherence probably holds over large regions of the Local Supercluster.
Sample of 97 spirals with accurate redshifts Further sample of 117 spirals Name Galaxy designation (NGC, IC or UGC) --- Type Numerical type --- cz Heliocentric redshift from BGFP catalogue number=1 In table2, data from BGFP catalogue (Bottinelli L., Gouguenheim L., Fouque P. and Paturel G., 1990, A&AS, 82, 391 Catalogue <VII/136>). In table8, data from Green Bank data, Tifft W.G., Cocke W.J., 1988, ApJS, 67,1 =1988ApJS...67....1T Tifft W.G., 1990, ApJS, 73, 603 =1990ApJS...73..603T Tifft W.G., 1992, ApJS, 79, 183 =1992ApJS...79..183T km/s GLAT Galactic longitude deg GLON Galactic longitude deg zgal Galactic redshift number=2 calculated for the solar vector (233km/s, 93deg, 2deg) - see text km/s Patricia Bauer CDS 1996 Feb 05 J_A+A_310_353.xml Four new active galaxies with steep soft X-ray spectra J/A+A/310/384 J/A+A/310/384 Optical brightness of 3 ROSAT Seyfert galaxies Four new active galaxies with steep soft X-ray spectra J Greiner R Danner N Bade G A Richter P Kroll S Komossa Astron. Astrophys. 310 384 1996 1996A&A...310..384G Active gal. nuclei Galaxies, optical Galaxies, photometry galaxies: active galaxies: individual (RX J1225.7+2055, RX J1239.3+2431) galaxies: individual (RX J1250.2+1923, RX J1257.5+2412) X-rays: general The printed version of this paper describes the X-ray and optical properties of four new active galaxies discovered in the ROSAT All-Sky Survey. While one object (RX J1257.5+2412) is identified as a BL Lac object, the other three (RX J1239.3+2431, RX J1225.7+2055, and RX J1250.2+1923) are narrow line Seyfert 1 galaxies. Three of these four objects are bright enough to be studied on archival photographic plates of Sonneberg Observatory. The present list contains the individual brightness measurements of these objects all of which turned out to be variable on timescales of weeks to years. Some lightcurves (long-term as well as short-term) are given in the printed version.
ROSAT RX J1225.7+2055 S10942 12 25.7 +20 55 RX J1257.5+2412 S10941 12 57.5 +24 12 RX J1239.3+2431 S10940 12 39.3 +24 31
Optical brightness estimates HJD Julian date of middle of exposure time. The exposure time ranges between 40-60 min. d Mag1 Brightness estimate for RX J1225.7+2055 mag n_Mag1 Comment on accuracy of brightness estimate of RX J1225.7+2055 number=1 No entry in the comment column means an accurate brightness estimate (error of +/-0.08 mag), while the five different signs have the following meanings: < denotes an upper limit, : denotes a slightly increased error (+/-0.14 mag), :: denotes an increased error (+/-0.20 mag), ? denotes an uncertain measurement, ?? denotes a doubtful measurement. --- Mag2 Brightness estimate for RX J1257.5+2412 mag n_Mag2 Comment on accuracy of brightness estimate of RX J1257.5+2412 number=1 No entry in the comment column means an accurate brightness estimate (error of +/-0.08 mag), while the five different signs have the following meanings: < denotes an upper limit, : denotes a slightly increased error (+/-0.14 mag), :: denotes an increased error (+/-0.20 mag), ? denotes an uncertain measurement, ?? denotes a doubtful measurement. --- Mag3 Brightness estimate for RX J1239.3+2431 mag n_Mag3 Comment on accuracy of brightness estimate of RX J1239.3+2431 number=1 No entry in the comment column means an accurate brightness estimate (error of +/-0.08 mag), while the five different signs have the following meanings: < denotes an upper limit, : denotes a slightly increased error (+/-0.14 mag), :: denotes an increased error (+/-0.20 mag), ? denotes an uncertain measurement, ?? denotes a doubtful measurement. --- Patricia Bauer CDS 1995 Dec 20 J_A+A_310_384.xml Lithium abundance in binaries of the Hyades open cluster J/A+A/310/879 J/A+A/310/879 Hyades binaries Lithium abundance in binaries of the Hyades open cluster D Barrado y Navascues J R Stauffer Astron. Astrophys. 310 879 1996 1996A&A...310..879B Photometry, UBV binaries: close open clusters and associations: individual (Hyades) stars: abundances stars: late-type We have derived accurate and homogeneous lithium abundances in 49 Main Sequence binary systems belonging to the Hyades open cluster by using a deconvolution method to determine individual magnitudes and colors for the primary and secondary components of the binary. The input parameters of the model are the observed Li equivalent width, the actual distance to the binary, the integrated apparent magnitude and the integrated colors of the binaries -BV(RI)_K_. We show that the general behavior is the same in binaries and in single stars (Li is depleted faster in K stars than in G stars and there is a deep dip for mid-F stars). However, there is a larger scatter in the abundances of binary systems than in single stars. Moreover, in general, binary systems have an overabundance, which is more conspicuous in close binaries. In fact, there is a cut-off period, which can be estimated as P_orb_~9d. This value is in excellent agreement with the theoretical prediction of Zahn (1994).
*Deconvolution for the Hyades binaries Name Star name number=1 vB: van Bueren, 1952 BD: Donner Durchmusterung J: Johnson et al., 1968 vA: van Altena, 1969 --- n_Name Note on the star number=2 Individual notes: 1 ADS 2451. The photometry include the visual companion. Mason et al. (1993) estimated {DELTA}V=6.0mag. 2 Distance and spectral types from Strassmeier et al 1993. (B-V)_p_ was assigned according the spectral type. 3 {DELTA}V=1.75mag from Griffin & Gunn (1981). Probable triple system. 4 {DELTA}V=0.5mag from Griffin & Gunn (1981). 5 (B-V)_p_ measured directly during the eclipse (Schiller & Milone 1987). 6 {DELTA}V=0.35mag from Batten & Wallerstein (1973). It could have an additional component. 7 {DELTA}V=1.12mag from Griffin et al. (1982). 8 ADS 3135. {DELTA}V=1.0mag from Wickes (1975). V={7.24+8.24} from Peterson & Solenski (1987). Visual companion included in the photometry. 9 Boesgaard & Tripicco (1986) obtained {DELTA}V=0.056mag from the ratio between spectral lines. 10 Visual component included in the photometry. 11 ADS 3169. Visual component included in the photometry. 12 The contribution from the secondary is apparently negligible. 13 The contribution from the secondary is apparently negligible. 14 {DELTA}V=2.0mag from Griffin et al. (1985). 15 {DELTA}V=0.45mag from Peterson & Solenski (1987). V={7.01+7.46}. The visual companion is included in the photometry. 16 ADS 3210. {DELTA}V=0.50mag from Heintz (1969). V={8.06+8.56} from Peterson & Solenski (1987). The visual companion is included in the photometry. 17 V_obs_=9.03 from Mermilliod (1976). 18 ADS 3248. {DELTA}V=0.65mag from Dombrowski (1991). Triple system. The inner pair is the SB2. The whole deconvolution is {F7 V + K0 V} + F9 V, V = {3.644+5.655} +4.136,(B-V) = {0.481+0.819} + 0.545 19 The contribution from the secondary is apparently negligible. 20 The visual companion is not included in the photometry. 21 Strassmeier et al. (1993) give M_V_=6.8mag, D=16.7 pc and dK5e. Apparent magnitude from Eggen & Greenstein (1965). Distance from Borgman & Lippicott (1983). Another possibility for the deconvolution could be (B-V)_calc_=1.085, (B-V)_p_=1.068, (B-V)_s_=1.7, M_calc_=6.648, M_p_=6.687, M_s_=10.291, (1+{alpha})=1.036, {DELTA}V=3.6mag. 22 {DELTA}V=2.0, Griffin et al. (1985). 23 The deconvolution was taken from Griffin et al. (1985). 24 The contribution from the secondary is apparently negligible. 25 {DELTA}V=0.14mag, Spectral types, distance and deconvolution from Griffin et al. (1985). 26 V_primary_=10.28, V_secondary_=10.59, Griffin & Gunn (1978). Distance from Schwan (1991), Spectral types from Strassmeier et al. (1993) 27 {DELTA}V=0.2mag from Thorburn et al. (1993) from the ratio between CaI6718A. V_obs_=7.34, 7.59, 7.71, 7.73 and 8.18, from Schwan (1991), Mermilliod (1976), Stern (1994) and Mason et al. (1993), respectively. 28 ADS 3475. Also (B-V)_obs_=0.50 from Mermilliod (1976). {DELTA}V=0.19mag from Dombrowski (1991). The visual component is included in the photometry. 29 ADS 3483. Triple system (Griffin et al. 1985): {F5 V + G8 V} + G4 V, V = {3.4 + 5.58} + 4.96, (B-V) = {0.42 + 0.81} + 0.68 --- B-Vobs Observed system B-V colour index mag l_B-V1 Flag on B-V1 --- B-V1 (B-V) colour index of the primary component mag B-V2 (B-V) colour index of the secondary component mag Dist Distance pc u_Dist Uncertainty flag on distance --- n_Dist Note on distance number=3 a: Distance estimated from the photometry. b: Calculated from V and <m-M>_binary_=3.40 --- MVmag Observed absolute V magnitude mag n_MVmag Note on MVmag number=3 a: Distance estimated from the photometry. b: Calculated from V and <m-M>_binary_=3.40 --- MVmag1 Absolute V magnitude of the primary mag MVmag2 Absolute V magnitude of the secondary mag Vmag Apparent V magnitude mag Sp Spectral type of the binary --- Sp1 Spectral type of the primary component --- Sp2 Spectral type of the secondary component --- Bin Binarity type --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 Feb 09 D. Barrado y Navascues <dbarrado@cfa.harvard.edu> J_A+A_310_879.xml Detection of C_2_, CN, and NaID absorption in the AGB remnant of HD 56126 J/A+A/310/893 J/A+A/310/893 C_2_ Phillips and CN Red bands in HD 56126 Detection of C_2_, CN, and NaID absorption in the AGB remnant of HD 56126 E J Bakker L B F M Waters H J G L M Lamers N R Trams F L A Van der Wolf Astron. Astrophys. 310 893 1996 1996A&A...310..893B Atomic physics Equivalent widths circumstellar matter molecular processes stars: AGB and post-AGB stars: individual (HD 56126) We present the detection of molecular absorption lines in the optical spectrum of the post-AGB star HD 56126. The C_2_ Phillips A^1^{PI}_u_-X^1^{SIGMA}^+^_g_(1,0), (2,0), and (3,0); Swan d^3^{PI}_g_-a^3^{PI}_u_(0,0) and (1,0); and CN Red system A^2^{PI}-X^2^{SIGMA}^+^ (1,0), (2,0), (3,0), and (4,0) bands have been identified. From the identification of the molecular bands we find an expansion velocity of 8.5+/-0.6km/s independent of excitation condition or molecular specie. On the basis of the expansion velocity, rotational temperatures, and molecular column densities we argue that the line-forming region is the AGB remnant. This is in agreement with the expansion velocity derived from the CO lines. We find column densities of logN_C_2__=15.3+/-0.3cm^-2^ and logN_CN_=15.5+/-0.3cm^-2^, and rotational temperatures of T_rot_=242+/-20K and T_rot_=24+/-5K respectively for C_2_ and CN. By studying molecular line absorption in optical spectra of post-AGB stars we have found a new tracer of the AGB remnant. From comparison with the results of CO and IR observations it is possible to obtain information on non-spherical behavior of the AGB remnant. Using different molecules with different excitation conditions it should be possible to study the AGB remnant as a function of the distance to the star, and thus as a function of the evolutionary status of the star on the AGB.
HD 56126 07 16 10.2 +09 59 48
(1,0) C_2_ Phillips band (2,0) C_2_ Phillips band (3,0) C_2_ Phillips band B(J'') Line identification --- LabLambda Laboratory wavelength in air 0.1nm ObsLambda Observed wavelength 0.1nm Wlambda Observed equivalent width 0.1pm f(J'J'')10+4 Oscillator strength --- N(J'') Column density 10+12cm-2 Rem Remarks --- (1,0) CN Red band (2,0) CN Red band (3,0) CN Red band B Line identification, branch name --- J'' Rotational quantum number, total angular momentum including spin number=1 Herzberg G., 1950 "Molecular spectra and molecular structure. I. Spectra of Diatomic molecules.", second edition. For CN, N''=J''+/-1/2 --- N'' Rotational quantum number, total angular momentum excluding spin number=1 Herzberg G., 1950 "Molecular spectra and molecular structure. I. Spectra of Diatomic molecules.", second edition. For CN, N''=J''+/-1/2 --- LabLambda Laboratory wavelength of transition in air 0.1nm ObsLambda Observed wavelength 0.1nm n_ObsLambda b=blend, N=NO --- W Observed equivalent width 0.1pm f(J'J'')10+4 Oscillator strength --- N(N''J'') Column density 10+12cm-2 Rem Remarks --- Patricia Bauer CDS 1996 Mar 23 J_A+A_310_893.xml The ESO Nearby Abell Cluster Survey. I. Description of the dataset and definition of physical systems J/A+A/310/8 J/A+A/310/8 The ESO Nearby Abell Cluster Survey I. The ESO Nearby Abell Cluster Survey. I. Description of the dataset and definition of physical systems P Katgert A Mazure J Perea R den Hartog M Moles O Le Fevre P Dubath P Focardi G Rhee B Jones E Escalera A Biviano D Gerbal G Giuricin Astron. Astrophys. 310 8 1996 1996A&A...310....8K J/A+A/310/31 : ENACS. Part II. Clusters, galaxy Redshifts cosmology: observations dark matter galaxies: clusters: general galaxies: distances and redshifts We describe the results of the ESO Key-programme on "Structure and Dynamics of Rich Galaxy Clusters" (which we will henceforth refer to as the ESO Nearby Abell Cluster Survey - or ENACS). We discuss the sample of clusters for which data were obtained, and the observational programme of spectroscopy and photometry that we carried out. The final database contains a total of 5634 galaxies in the directions of 107 clusters from the catalogue by Abell, Corwin and Olowin 1989 (ACO hereafter) with richness R>=1 and mean redshifts z<=0.1.
Properties of the 220 systems with N>= 4 found in the 107 lines of sight towards the ACO clusters in the ESO Nearby Abell Cluster Survey (ENACS) Abell Abell number of cluster --- Ngal Number of galaxies in system (ENACS) --- zmin Lowest galaxy redshift in the system (ENACS) --- zmax Highest galaxy redshift in the system (ENACS) --- zmean Mean redshift of the system (ENACS) --- Nz Number of redshifts (literature) --- zmean2 Mean redshift of system (literature) -- Ref reference to literature data (see paper) --- Patricia Bauer CDS 1996 Apr 24 Peter Katgert <katgert@strw.LeidenUniv.nl> J_A+A_310_8.xml Quantitative analysis of carbon isotopic ratios in carbon stars. I. 62 N-type and 15 SC-type carbon stars. J/A+A/310/933 J/A+A/310/933 C isotopic ratio in N- and SC-type stars Quantitative analysis of carbon isotopic ratios in carbon stars. I. 62 N-type and 15 SC-type carbon stars. K Ohnaka T Tsuji Astron. Astrophys. 310 933 1996 1996A&A...310..933O Photometry, CCD Stars, carbon stars: abundances stars: AGB and post-AGB stars: atmospheres stars: carbon stars: evolution stars: fundamental parameters We present a result of quantitative analysis of ^12^C/^13^C ratios in 62 N-type and 15 SC-type carbon stars. By the use of CCD as a detector we can obtain spectra of resolution ~20,000 with enough signal-to-noise ratios for a large number of carbon stars, for which ^12^C/^13^C ratios have not yet been derived. Carbon isotopic ratios are determined from lines of the CN red system around 8000A, based on the iso-intensity method and line-blanketed model atmospheres. The average of ^12^C/^13^C ratios in 62 N-type carbon stars is found to be 27+/-11 (standard deviation). The majority of the N-type carbon stars studied (about 85%) are found to have ^12^C/^13^C ratios less than 40, and the number of stars which have ^12^C/^13^C ratios larger than 40 is found to be relatively small. This result shows a marked contrast to some of the previous results that have shown the opposite distribution, namely, ^12^C/^13^C ratios mostly larger than 40 in N-type carbon stars. The average of ^12^C/^13^C ratios in 15 SC-type carbon stars is found to be 22+/-14 (standard deviation). Most of the SC-type carbon stars studied are found to have ^12^C/^13^C ratios larger than 10, while only three of them turn out to be ^13^C-rich. This is in contrast with the earlier classification based on low resolution spectra which classified them as J-type, that is, ^13^C-rich. The earlier temperature scale which classified SC-type carbon stars as the latest (C8-9) based on their strong NaI D lines can not be necessarily justified. The strong NaI D lines of SC stars should be attributed to the peculiar atmospheric structure due to C/O ratios very near to unity. The resulting ^12^C/^13^C ratios are partly consistent with the scenario in which M giants evolve through SC-type to N-type carbon stars, as ^12^C produced during the helium shell flash is added to the envelope.
Summary of the observations of 66 N-type carbon stars Summary of the observations of 19 SC-type carbon stars GCCGCS Designation in "A General Catalogue of Cool Galactic Carbon Stars", Stephenson (1989) (Catalogue <III/156>) --- CCCS Designation in "A General Catalogue of Cool Carbon Stars", Stephenson (1973) --- n_CCCS A ')' indicates that the designation is in "A General Catalog of S stars", Stephenson (1976) (Catalogue <III/168>) --- Name Star Name --- C-Class C-Classification, Yamashita (1972, 1975) --- Vmag V magnitude or lowest V magnitude if interval mag n_Vmag A '-' indicates an interval of magnitudes --- l_Vmag2 Limit flag on Vmag2 --- Vmag2 Upper V magnitude if interval mag Obs Date of observations for two wavelength --- S/N Signal-to-noise ratio --- table1.tex LaTeX version of table1 table2.tex LaTex version of table2 Patricia Bauer CDS 1996 Mar 26 J_A+A_310_933.xml Forty days in the life of CF Tucana (=HD 5303). The longest stellar X-ray flare observed with ROSAT J/A+A/311/211 J/A+A/311/211 X-ray flare of CF Tuc Forty days in the life of CF Tucana (=HD 5303). The longest stellar X-ray flare observed with ROSAT M Kuerster J H M M Schmitt Astron. Astrophys. 311 211 1996 1996A&A...311..211K Stars, flare binaries: eclipsing stars: activity stars: coronae stars: flare stars: individual (CF Tuc) stars: late-type stars: rotation Solar abundance fits to the quiescent spectra 1-3 and 20-35 were made with a two-component thermal plasma (model 1a) whereas sub-solar abundance fits to the quiescent spectra were made with a one-component thermal plasma (model 2a). Modifications of these models were used for the flare spectra 4-19 in order to account for the `quiescent background'. Thus solar abundance fits to the flare spectra were made with a thermal plasma of two variable components plus two components kept constant at the average quiescent values T_qu,cool=2.46*10^6K, EM_qu,cool=0.49*10^53cm^-3, T_qu,hot =17.8*10^6K, EM_qu,hot=1.95*10^53cm^-3, and z=1.00 (model 1b). Sub-solar abundance fits to the flare spectra were made with a plasma of one variable component plus one component kept constant at the average quiescent values T_qu=13.0*10^6K, EM_qu=5.20*10^53cm^-3, and z=0.10 (model 2b). In both cases the mean values of spectra 3, and 20-35 were used to account for the quiescent emission.
HD 5303 CF Tuc 00 53 04.8 -74 39 07
Raymond-Smith model fits with solar and sub-solar metal abundances, z=1.0 and z=0.1. Sq Number of the spectrum --- State Emission state as inferred from the light curve number=1 qu/f = high-level quiescent emission or possible flare, qu = low-level quiescent emission, f-r = flare rise, f-p = flare peak, d-r = rapid flare decay, d-h = decay halt, d-s = slow flare decay. --- HJD Heliocentric Julian day d NH1 Hydrogen column density, model 1 number=2 Model 1: 2-component model (1a/1b) with metallicity z=1.0 10+19cm-2 e(NH1)u Error in NH1, upper limit 10+19cm-2 e(NH1)l Error in NH1, lower limit 10+19cm-2 EMcool Emission measure of the cooler plasma component, model 1 number=2 Model 1: 2-component model (1a/1b) with metallicity z=1.0 10+53cm-3 e(EMcool)u Error in EMcool, upper limit 10+53cm-3 e(EMcool)l Error in EMcool, lower limit 10+53cm-3 Tcool temperature of the cooler plasma component, model 1 number=2 Model 1: 2-component model (1a/1b) with metallicity z=1.0 10+6K e(Tcool)u Error in Tcool, upper limit 10+6K e(Tcool)l Error in Tcool, lower limit 10+6K EMhot Emission measure of the hotter plasma component, model 1 number=2 Model 1: 2-component model (1a/1b) with metallicity z=1.0 10+53cm-3 e(EMhot)u Error in EMhot, upper limit 10+53cm-3 e(EMhot)l Error in EMhot, lower limit 10+53cm-3 Thot Temperature of the hotter plasma component, model 1 number=2 Model 1: 2-component model (1a/1b) with metallicity z=1.0 10+6K e(Thot)u Error in Thot, upper limit 10+6K e(Thot)l Error in Thot, lower limit 10+6K Chi21 Reduced chi-square of the fit, model 1 number=2 Model 1: 2-component model (1a/1b) with metallicity z=1.0 --- f_Chi21 Number of degrees of freedom of chi2 --- NH2 Hydrogen column density, model 2 number=3 Model 2: 1-component model (2a/2b) with z=0.1 10+19cm-2 e(NH2)u Error in NH2, upper limit 10+19cm-3 e(NH2)l Error in NH2, lower limit 10+19cm-3 EM Emission measure, model 2 number=3 Model 2: 1-component model (2a/2b) with z=0.1 10+53cm-3 e(EM)u Error in EM, upper limit 10+53cm-3 e(EM)l Error in EM, lower limit 10+53cm-3 T Temperature, model 2 number=3 Model 2: 1-component model (2a/2b) with z=0.1 10+6K e(T)u Error in T, upper limit 10+6K e(T)l Error in T, lower limit 10+6K Chi22 Reduced chi-square of the fit, model 2 number=3 Model 2: 1-component model (2a/2b) with z=0.1 --- f_Chi22 Number of degrees of freedom --- Patricia Bauer CDS 1996 Mar 01 Martin Kuerster, <mak@rosat.mpe-garching.mpg.de> J_A+A_311_211.xml Spectro-photometric evolution of elliptical galaxies. II. Models with infall. J/A+A/311/361 J/A+A/311/361 Evolution models of elliptical galaxies. II. Spectro-photometric evolution of elliptical galaxies. II. Models with infall. R Tantalo C Chiosi A Bressan F Fagotto Astron. Astrophys. 311 361 1996 1996A&A...311..361T Models, evolutionary Photometry, UBVRIJKLMNH galaxies: elliptical and lenticular, cD galaxies: evolution galaxies: stellar content In this paper we present new chemo-spectro-photometric models of elliptical galaxies in which infall of primordial gas is allowed to occur. They aim to simulate the collapse of a galaxy made of two components, i.e. luminous material and dark matter. The mass of the dark component is assumed to be constant in time, whereas that of the luminous material is supposed to accrete at a suitable rate. They also include the effect of galactic winds powered by supernova explosions and stellar winds from massive, early-type stars. The models are constrained to match a number of properties of elliptical galaxies, i.e. the slope and mean colours of the colour-magnitude relation (CMR), V versus (V-K), the UV excess as measured by the colour (1550-V) together with the overall shape of the integrated spectral energy distribution (ISED) in the ultraviolet, the relation between the Mg_2_ index and (1550-V), the mass to blue luminosity ratio M/L_B_ as a function of the B luminosity, and finally the broad-band colours (U-B), (B-V), (V-I), (V-K), etc. The CMR is interpreted as a mass-metallicity sequence of old, nearly coeval objects, whose mean age is 15Gyr. Assuming the law of star formation to be proportional to M_g_^k^(t) with k=1, the rate of star formation as function of time starts small, grows to a maximum, and then declines thus easily avoiding the excess of metal-poor stars found by BCF with the closed-box scheme (the analog of the G-Dwarf Problem in the solar vicinity). Owing to their stellar content, infall models can easily reproduce all the basic data of the galaxies under examination. As far as the UV excess is concerned, the same sources proposed by BCF are found to hold also with the infall scheme. H-HB and AGB manque stars of high metallicity play the dominant role, and provide a robust explanation of the correlation between the (1550-V) colour and the luminosity, mass and metallicity of the galaxies. Furthermore, these models confirm the potential of the (1550-V) colour as an age indicator in cosmology as already suggested by BCF. In the rest frame of a massive and metal-rich elliptical galaxy, this colour suffers from one major variation: at the onset of the so-called H-HB and AGB-manque stars (age about 5.6Gyr). This transition occurs at reasonably small red-shifts and therefore could be detected with the present-day instrumentation.
Integrated colors of single stellar populations Z Metallicity --- Age Age Gyr Mv Integrated absolute visual magnitude mag Mbol Integrated absolute bolometric magnitude mag BC Bolometric correction mag U-B U-B integrated color mag B-V B-V integrated color mag V-R V-R integrated color mag R-I R-I integrated color mag V-J V-J integrated color mag V-K V-K integrated color mag V-L V-L integrated color mag V-M V-M integrated color mag V-N V-N integrated color mag 1550-V 1550-V integrated color defined as in Burstein et al. 1988 mag Patricia Bauer CDS 1996 Apr 04 J_A+A_311_361.xml ROSAT observations of BL Lacertae objects. J/A+A/311/384 J/A+A/311/384 ROSAT observations of BL Lacertae objects ROSAT observations of BL Lacertae objects. G Lamer H Brunner R Staubert Astron. Astrophys. 311 384 1996 1996A&A...311..384L BL Lac objects X-ray sources BL Lacertae objects: general galaxies: active radio continuum: galaxies X-rays: galaxies We present soft X-ray spectra of 74 BL Lacertae objects observed with the PSPC detector on board of the ROSAT satellite. The sample contains all BL Lac objects detected during the pointed observation phase as a target or serendipitously. We have investigated the soft X-ray and broad band spectral properties and discuss the consequences for the X-ray emission processes. For the first time a clear dependence of the X-ray spectral steepness on the radio to X-ray spectral energy distribution is found: {alpha}_rx_ and {alpha}_x_ are correlated in the X-ray selected (XBL) subsample and anticorrelated in the radio selected (RBL) subsample. The objects with intermediate {alpha}_rx_ values thus do have the steepest soft X-ray spectra. Simulated PSPC spectra based on a set of simple two component multifrequency spectra are in good agreement with the measurements and suggest a broad range of synchrotron cutoff energies. We have calculated synchrotron self-Compton beaming factors for a subsample of radio bright objects and find a correlation of the beaming factors {delta}_IC_ with {alpha}_rx_ and {alpha}_x_. The most extreme RBL objects are very similar to flat spectrum radio quasars in all their broad band and X-ray properties.
ROSAT
List of PSPC observations Name Object name --- ROR ROSAT observation request (ROR) number --- n_ROR '-' when two ROR numbers --- ROR2 Second ROR number --- Date Completed date --- Exp Exposition time s Counts Net counts --- e_Counts rms uncertainty on Counts --- X-ray and broad band spectra Name Object name --- NH,gal Galactic hydrogen column density 10+20cm-2 n_NH,gal Note on NH,gal number=1 a: Elvis et al. 1989, other values: Stark et al. 1992 --- NH,fit Fitted hydrogen column density 10+20cm-2 e_NH,fit rms uncertainty on NH,fit 10+20cm-2 F1keV Flux at 1 keV uJy alpha Spectral index between .1kev and 2.4keV --- e_alpha rms uncertainty on alpha --- alpha_rx_ X-ray spectral index --- delta_IC_ Inverse Compton beaming factor --- Patricia Bauer CDS 1996 Mar 26 J_A+A_311_384.xml UBV-JHKLM photometry of CH Cygni over 1978-1995: dust properties and doubts on the triple star model. J/A+A/311/484 J/A+A/311/484 CH Cyg 1991-1995 UBV-JHKLM photometry UBV-JHKLM photometry of CH Cygni over 1978-1995: dust properties and doubts on the triple star model. U Munari B F Yudin E A Kolotilov T V Tomov Astron. Astrophys. 311 484 1996 1996A&A...311..484M Photometry, UBVRIJKLMNH binaries: symbiotic infrared: stars stars: individual (CH Cyg) We present new UBV-JHKLM photoelectric photometry of the symbiotic binary CH Cyg covering the period 1991-1995, which extend our monitoring started in 1978. The large and highly homogeneous set of data that we have accumulated in the last eighteen years is reviewed and discussed. By July 1995 the outbursting component has returned to the same conditions which characterized the previous minimum in 1988-1989. In J, H, K CH Cyg shows a long term modulation that can be fitted with a sinusoid of 32 year period. It may be a dust obscuration event similar to those known to undergo in symbiotic Miras. The cool giant exhibits in the infrared a variability of large amplitude, best described as chaotic-like. The only detectable periodicity is 1980 days. The photometric properties of the cool giant denounce a clear partnership with the spheroidal component of the Galaxy. This lowers the estimated distance to ~120pc and the cool giant mass to ~1.0M_{sun}_. Several episodes of dust condensation in the wind of the giant are identified. One is in full progress at the time of writing. The dust condensation temperature is found to be ~1,000K. The condensed dust grains absorb selectively in the infrared but are large enough to absorb neutrally in the UBV wavelength region. There is no evidence for dust condensing in an hypothetical wind or ejected material from the outbursting white dwarf. The recently proposed triple-star model for CH Cyg is confronted with photometric observations. Several serious discrepancies are outlined and individually discussed. We believe that, without additional evidences and careful modelling, the triple star model cannot survive the comparison with the photometric observations. The low amplitude (2.6km/s) and periodic (756 days) radial velocity variations apparently do not trace an orbital motion. They may be due to one of the many superimposed pulsation modes of the highly variable M giant.
CH Cyg HD 182917 BD+49 2999 19 24 33.0 +50 14 30
1991-1995 CH Cyg UBV photoelectric photometry JD Julian date d Umag U magnitude mag Bmag B magnitude mag Vmag V magnitude mag 1991-1995 CH Cyg JHKLM photoelectric photometry JD Julian date d Jmag J magnitude mag Hmag H magnitude mag Kmag K magnitude mag Lmag L magnitude mag Mmag M magnitude mag table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 Patricia Bauer CDS 1996 Apr 02 J_A+A_311_484.xml The properties of W Ursae Majoris contact binaries: new results and old problems J/A+A/311/523 J/A+A/311/523 Photometry of W UMa The properties of W Ursae Majoris contact binaries: new results and old problems C Maceroni F van't Veer Astron. Astrophys. 311 523 1996 1996A&A...311..523M Binaries, eclipsing Magnitudes Reddening Spectral types binaries: close stars: evolution stars: mass-loss The physical properties of W UMa binary systems are revisited on the basis of the observational data published in the last decade and of the recent theoretical studies on angular-momentum-loss-driven secular evolution. The absolute elements (masses, radii, luminosities) are derived by an inference method and a calibration based on the available high quality spectroscopic orbits. The derived age (8Gy) agrees with the estimate of Guinan and Bradstreet from space motions. The analysis of the resulting physical parameters shows little correlation between the standard classification in A and W subtype (first proposed by Binnendijk (1970) and only related to the light curve morphology) and the evolutionary status and origin of the systems. Most A-subtype systems seem to have no evolutionary link with W-subtype ones. The relation between total mass and mass ratio for the "bona fide" sample also suggests that mass loss from the system may play an important role.
Basic observational data of W UMa binaries No Sequential number number=1 Systems denoted by sequential numbers from 1 to 48 are classified as W-subtype, the others as A-subtype (Binnendijk L, 1970, Vistas in Astr. 12, 217). Within each sub-type systems are ordered according to increasing orbital period. The values presented derive from the papers on individual systems listed in the original paper (Table 2), or from the General Catalogue of Variable Stars 4th ed. (Khopolov P.N. et al. 1985, Nauka Publ. Co., Moscow, Catalogue <II/195>) and the Eight Catalogue of the orbital elements of spectroscopic binary systems (Batten A.H., Fletcher J.M, MacCarthy D.G., 1989 Publ. D.A.O. vol XVII, Catalogue <V/64>). --- Name Star name --- Per Orbital period d MaxMag Maximum magnitude mag MinMag Minimum magnitude mag MagType Type of magnitudes --- Sp Spectral type(s) --- B-V B-V color index mag E(B-V) Reddening mag u_E(B-V) Uncertainty flag on E(B-V) --- Patricia Bauer CDS 1996 Apr 09 Carla Maceroni <maceroni@coma.mporzio.astro.it> J_A+A_311_523.xml Observations and ephemerides of the faint satellites of Jupiter J/A+A/311/710 J/A+A/311/710 Faint Jovian satellites ephemerides Observations and ephemerides of the faint satellites of Jupiter P Rocher J Chapront Astron. Astrophys. 311 710 1996 1996A&A...311..710R Ephemerides Planets ephemerides planets and satellites: individual (Jupiter) The observations of the faint satellites of Jupiter J6, J7, J8 and J9 have been collected. Numerical integrations have been performed and fitted to ancient and modern observations. Ephemerides of the equatorial jovicentric rectangular coordinates of the satellites are presented under the form of Poisson series, covering 150 years from 1900. Numerical tools (tables and softwares) are provided to the users for a practical reconstruction of the ephemerides.
Observations of J6 Observations of J7 Observations of J8 Observations of J9 o_Obs Number of observations --- OBSyr Date of observation in UT (year) yr OBSm Date of observation in UT (month) --- OBSd Date of observation in UT (day) d RAh Topocentric right ascension of observation h RAm Topocentric right ascension of observation min RAs Topocentric right ascension of observation s DE- Declination sign --- DEd Topocentric declination of observation deg DEm Topocentric declination of observation arcmin DEs Topocentric declination of observation arcsec l_O-Ca Limit flag on O-Ca --- O-Ca Observed - Calculed alpha * cos(delta) arcsec n_O-Ca '*' = rejected observation in alpha --- l_O-Cd Limit flag on O-Cd --- O-Cd Observed - Calculed delta arcsec n_O-Cd '*' = rejected observation in delta --- Obs Observatory code (see file Code.txt) --- Ref References of observation : code of publication volume, page (see file Code.txt) --- Observatory codes Obs Observatory code --- Name Observatory name --- L Geocentric longitude in fraction of day (positive towards the west and negative towards the east). d ro*sin(phi') ro * sin(phi') number=1 ro : radial geocentric distance phi' : geocentric latitude. --- ro*cos(phi') ro * cos(phi') number=1 ro : radial geocentric distance phi' : geocentric latitude. --- install.txt Procedure of installation of faintsat.zip Patricia Bauer CDS 1996 Apr 01 P. Rocher, J. Chapront Bureau des Longitudes, CNRS URA 707 77, avenue Denfert-Rochereau 75014, Paris, France Tel : (33) 1 40 51 22 72 (33) 1 40 51 22 71 Fax : (33) 1 46 33 28 34 Mail : <rocher@bdl.fr> Jean.Chapront@bdl.fr J_A+A_311_710.xml Corrections and new developments in rigid Earth nutation theory. I. Lunisolar influence including indirect planetary effects. J/A+A/312/1017 J/A+A/312/1017 Coefficients of rigid Earth nutation. I. Corrections and new developments in rigid Earth nutation theory. I. Lunisolar influence including indirect planetary effects. J Souchay H Kinoshita Astron. Astrophys. 312 1017 1996 1996A&A...312.1017S J/A+AS/116/473 : Nutation modeling and VLBI observations (Souchay+, 1996) Kinoshita H. and Souchay J., 1990, Celest. Mech. 48, 187 Earth celestial mechanics, stellar dynamics Earth reference systems The tables of nutation as given by Kinoshita & Souchay (1990) have been constructed with use of the value of the general precession in longitude as adopted by the IAU1976 (Lieske et al. 1977). The recent observations agree to give a correction of about 0.3"/cy. to this last value. Because of the interaction between the precession and the nutation for a rigid Earth model, it became necessary to use an updated value of p_A_, that is to say: p_A_=5028.7700"/cy and to recalculate the largest coefficients of nutation influenced by this change. This is one of the aim of this paper. Moreover, we study a new contribution to the nutation not included in the preceding studies, which are due to the periodic oscillations of the ecliptic. We also calculate the planetary tilt-effect on the nutation pointed out by Williams (1994), which was not included in Kinoshita & Souchay (1990). At last all the coefficients of the nutation for a rigid-Earth model have been recalculated, with an improved threshold of the potential (5x10^-10^). We give final tables showing all the coefficients subject to some change with respect to Kinoshita & Souchay (1990), for the lunisolar part, including the indirect planetary effects. Only the direct action of the planets on the nutation and the influence of the J_3_ geopotential is not studied here. They will be the subject of a next paper. At last a new value of the dynamical ellipticity of the Earth is calculated in the following: H_D_=0.0032737548.
Coefficients of rigid Earth nutation coming from the new contribution due to the small periodic oscillations of the ecliptic, up to 0.001 mas, in longitude Coefficients of rigid Earth nutation coming from the new contribution due to the small periodic oscillations of the ecliptic, up to 0.001 mas, in obliquity Ve Venus nutation coefficient --- Ea Earth nutation coefficient --- Ma Mars nutation coefficient --- Ju Jupiter nutation coefficient --- Sa Saturn nutation coefficient --- pA General precession in longitude 10-2arcsec/yr D D Delaynay argument nutation coefficient --- F F Delaynay argument nutation coefficient --- l l Delaynay argument nutation coefficient --- Omega Omega nutation coefficient --- P Period nutation coefficient yr Sin Sinus nutation coefficient mas Cos Cosinus nutation coefficient mas Coefficients of rigid Earth nutation coming from the indirect planetary contribution, solar part, up to 0.005 mas, in longitude Coefficients of rigid Earth nutation coming from the indirect planetary contribution, solar part, up to 0.005 mas, in obliquity Ve Venus nutation coefficient --- Ea Earth nutation coefficient --- Ma Mars nutation coefficient --- Ju Jupiter nutation coefficient --- Sa Saturn nutation coefficient --- pA Precession rate nutation coefficient 10-2arcsec/yr P Period nutation coefficient yr Sin New calculated sinus nutation coefficient 0.01mas Cos New calculated cosinus nutation coefficient 0.01mas SinKS KS calculates sinus nutation coefficient 0.01mas CosKS KS calculated cosinus nutation coefficient 0.01mas Note Note on the absolute differences with the respective value in the tables of Kinoshita and Souchay (1990) number=1 "*" indicates that the absolute difference is between 0.1 and 0.5mas "**" between 0.5 and 1.0mas "***" bigger than 1.0mas --- Coefficients of rigid Earth nutation coming from the indirect planetary contribution, lunar part, up to 0.005 mas, in longitude Coefficients of rigid Earth nutation coming from the indirect planetary contribution, lunar part, up to 0.005 mas, in obliquity Ve Venus nutation coefficient --- Ea Earth nutation coefficient --- Ma Mars nutation coefficient --- Ju Jupiter nutation coefficient --- Sa Saturne nutation coefficient --- D D Delaunay argument nutation coefficient --- F F Delaunay argument nutation coefficient --- l l Delaunay argument nutation coefficient --- Omega Omega nutation coefficient --- P Period nutation coefficient yr Sin New calculated sinus nutation coefficient 0.01mas Cos New calculated cosinus nutation coefficient 0.01mas SinKS KS calculated sinus nutation coefficient 0.01mas CosKS KS calculated cosinus nutation coefficient 0.01mas Note Comparison with the respective value of Kinoshita and Souchay (1990) number=1 "*" indicates that the absolute difference is between 0.1 and 0.5mas "**" between 0.5 and 1.0mas "***" bigger than 1.0mas --- table51.tex TeX version of table51 table52.tex TeX version of table52 table61.tex TeX version of table61 table62.tex TeX version of table62 Patricia Bauer CDS 1996 Mar 28 J_A+A_312_1017.xml Comparison of the Carlsberg optical references frame with the International celestial reference frame J/A+A/312/1031 J/A+A/312/1031 Positions & proper motions of radio stars Comparison of the Carlsberg optical references frame with the International celestial reference frame R W Argyle O H Einicke J D H Pilkington L V Morrison C Fabricius L Helmer Astron. Astrophys. 312 1031 1996 1996A&A...312.1031A I/213 : CMC8 (8th Carlsberg Meridian Catalog, 1994) I/205 : CMC7 (7th Carlsberg Meridian Catalogue, 1993) I/189 : CMC6 (6th Carlsberg Meridian Catalogue, 1992) I/170 : CMC5 (5th Carlsberg Meridian Catalogue, 1991) I/147 : CMC4 (4th Carlsberg Meridian Catalogue, 1989) Nebulae Positional data astrometry references frames The optical positions of 63 extragalactic nebulae measured in the frame defined by the annual series of Carlsberg Meridian Catalogues Nos 1-8 are compared with their VLBI radio positions in the International Celestial Reference Frame. The differences between these radio and optical positions are interpreted as showing the global distortion of the Carlsberg optical frame, which is linked to that of the FK5. North of the equator the Carlsberg optical frame is within 0.05" of the ICRF; but south of the equator it deviates by 0.07" in right ascension and 0.10" in declination. The general form of the deviations follow those of the FK5, which are revealed in a recent comparison of FK5 with a preliminary version of the Hipparcos catalogue (H30).
Carlsberg optical positions of ICRF sources and differences, radio minus optical Name Name of radio source (IAU nomenclature) --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEg Declination (2000) d DEm Declination (2000) arcmin DEs Declination (2000) arcsec Nplate Number of plates --- DRA Delta RA (radio-optical) arcsec DDE Delta DE (radio-optical) arcsec Carlsberg optical positions and proper motions of radio stars Name Name of radio star --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s pmRA Proper motion in right ascension s/yr EpRA-1900 Epoch of RA (1900+) yr DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec pmDE Proper motion in declination arcsec/yr EpDE-1900 Epoch of DE (1900+) yr DRA Delta RA(radio-optical) arcsec DDE Delta Dec(radio-optical) arcsec Patricia Bauer CDS 1996 Mar 11 R.W. Argyle, <merlp@ast.cam.ac.uk> J_A+A_312_1031.xml Determination of [Fe/H] from the light curves of RR Lyrae stars. J/A+A/312/111 J/A+A/312/111 [Fe/H] from RR Lyrae light curves Determination of [Fe/H] from the light curves of RR Lyrae stars. J Jurcsik G Kovacs Astron. Astrophys. 312 111 1996 1996A&A...312..111J Abundances, [Fe/H] Stars, variable globular clusters: general stars: abundances stars: horizontal-branch stars: oscillations stars: variables: other We present an accurate and robust method for the calculation of [Fe/H] from the light curves of RRab stars. The method introduces a considerable improvement relative to our previously published formulae. First of all, it uses an improved and extended data base for the light curves and more accurate, very recent iron abundances. Secondly, the new data base makes it possible to show that the basic relation between [Fe/H] and the Fourier parameters is linear and contains only the period and one of the Fourier phases, most importantly {phi}_31_. Last but not least, we derive interrelations among the Fourier parameters which help us to filter out peculiar stars where more caution is needed in accepting the calculated abundance. The applicability of the method is demonstrated on independent samples of globular cluster stars. Peculiarities encountered in Blazhko variables and in some other cases are also discussed. The Fourier decomposition is defined by the formula: V(t) = A0 + A1*sin(2*pi/P*(t-t0)+phi1) + A2*sin(2*pi*2/P*(t-t0)+phi2) +... + A15*sin(2*pi*15/P*(t-t0)+phi15) V(t) -- light curve in Johnson V P -- period t0 -- Epoch = 2400000.0
Fourier coefficients Name Star name number=1 Asterisks denote the stars where the different segments of the data sets were time and magnitude shifted. --- P Period d A0 Fourier coefficient A0 mag N Number of data point used --- Sigma standard deviation --- A1 Fourier coefficient A1 mag phi1 Fourier coefficient phi1 rad A2 Fourier coefficient A2 mag phi2 Fourier coefficient phi2 rad A3 Fourier coefficient A3 mag phi3 Fourier coefficient phi3 rad A4 Fourier coefficient A4 mag phi4 Fourier coefficient phi4 rad A5 Fourier coefficient A5 mag phi5 Fourier coefficient phi5 rad A6 Fourier coefficient A6 mag phi6 Fourier coefficient phi6 rad A7 Fourier coefficient A7 mag phi7 Fourier coefficient phi7 rad A8 Fourier coefficient A8 mag phi8 Fourier coefficient phi8 rad A9 Fourier coefficient A9 mag phi9 Fourier coefficient phi9 rad A10 Fourier coefficient A10 mag phi10 Fourier coefficient phi10 rad A11 Fourier coefficient A11 mag phi11 Fourier coefficient phi11 rad A12 Fourier coefficient A12 mag phi12 Fourier coefficient phi12 rad A13 Fourier coefficient A13 mag phi13 Fourier coefficient phi13 rad A14 Fourier coefficient A14 mag phi14 Fourier coefficient phi14 rad A15 Fourier coefficient A15 mag phi15 Fourier coefficient phi15 rad Patricia Bauer CDS 1996 Jan 30 J_A+A_312_111.xml The behaviour of the excess CaII H & K and Hepsilon emissions in chromospherically active binaries J/A+A/312/221 J/A+A/312/221 Excess CaII H&K emission in active binaries The behaviour of the excess CaII H & K and Hepsilon emissions in chromospherically active binaries D Montes M J Fernandez-Figueroa M Cornide E De Castro Astron. Astrophys. 312 221 1996 1996A&A...312..221M V/76 : A catalog of chromospherically Active Binaries Fernandez-Figueroa M.J., Montes D., De Castro E., Cornide M., 1994, ApJS 90, 433 =1994ApJS...90..433F Montes D., De Castro E., Fernandez-Figueroa M.J., Cornide M. 1995, A&AS 114, 287 =1995A&AS..114..287M Spectroscopy Stars, double and multiple binaries: close stars: activity stars: chromospheres stars: late-type stars: rotation In this work we analyze the behaviour of the excess CaII H & K and H_epsilon emissions in a sample of 73 chromospherically active binary systems (RS CVn and BY Dra classes), of different activity levels and luminosity classes. This sample includes the 53 stars analyzed by Fernandez-Figueroa et al. (1994) and the observations of 28 systems described by Montes et al. (1995). By using the spectral subtraction technique (subtraction of a synthesized stellar spectrum constructed from reference stars of spectral type and luminosity class similar to those of the binary star components) we obtain the active-chromosphere contribution to the CaII H & K lines in these 73 systems. We have determined the excess CaII H & K emission equivalent widths and converted them into surface fluxes. The emissions arising from each component were obtained when it was possible to deblend both contributions.
CaII H & K lines measures in the observed and subtracted spectrum (Group 1) CaII H & K lines measures in the observed and subtracted spectrum (Group 2) CaII H & K lines measures in the observed and subtracted spectrum (Group 3) Name Name --- Date Date mm/dd/yy "DD/MM/YY" phi [0/1] Orbital phase --- E H: hot C: cool T: Total --- SH/SC Weights for the hot and cool component --- EW(K) EW(K) by reconstruction of the absorption line 0.1nm EW(H) EW(H) by reconstruction of the absorption line 0.1nm EW(K)s EW(K) in the subtracted spectrum 0.1nm EW(H)s EW(H) in the subtracted spectrum 0.1nm EW(Hep)s EW(H_epsilon) in the subtracted spectrum 0.1nm EW(K)c EW(K) corrected 0.1nm EW(H)c EW(H) corrected 0.1nm EW(Hep)c EW(H_epsilon) corrected 0.1nm logF(K) log CaII K surface flux 10mW/m2/nm logF(H) log CaII H surface flux 10mW/m2/nm logF(Hep) log H_epsilon surface flux 10mW/m2/nm CaII H & K lines measures in the observed and subtracted spectrum (Single stars or components of visual binaries) HD HD number --- Name Name --- F(1.0)K Core flux at 1.0A for the K line in the normalized spectrum --- F(1.0)H Core flux 1.0A for the H line in the normalized spectrum --- EW(K) EW(K) by reconstruction of the absorption line 0.1nm EW(H) EW(H) by reconstruction of the absorption line 0.1nm EW(K)s EW(K) in the subtracted spectrum 0.1nm EW(H)s EW(H) in the subtracted spectrum 0.1nm EW(He)s EW(H_epsilon) in the subtracted spectrum 0.1nm logF(K) log CaII K surface flux (erg/cm2/s/A) 10mW/m2/nm logF(H) log CaII H surface flux 10mW/m2/nm logF(He) log CaII H-epsilon surface flux 10mW/m2/nm Patricia Bauer CDS 1996 May 20 David Monte <dmg@astro4.fis.ucm.es> J_A+A_312_221.xml New weak-line T Tauri stars in Taurus-Auriga J/A+A/312/439 J/A+A/312/439 New T Tauri stars in Taurus-Auriga New weak-line T Tauri stars in Taurus-Auriga R Wichmann J Krautter J H M M Schmitt R Neuhauser J M Alcala H Zinnecker R M Wagner R Mundt M F Sterzik Astron. Astrophys. 312 439 1996 1996A&A...312..439W J/A+A/297/391 : T Tauri stars ROSAT survey (Neuhaeuser+, 1995) Neuhauser R., Sterzik M.F., Schmitt J.H.M.M., Wichmann R., Krautter J. 1995b, =1995A&A...297..391N Stars, pre-main sequence X-ray sources stars: formation stars: late-type stars: pre-main sequence surveys X-rays: stars On the basis of the ROSAT All-Sky-Survey, a study of the Taurus-Auriga star forming region has been performed in order to search for hitherto undiscovered T Tauri stars. Our study covers an area of about 280 square degrees, located between 4^h^ and 5^h^ in right ascension and between 15deg and 34deg in declination. Identification of ROSAT All-Sky Survey sources in this area by means of optical spectroscopy revealed 2 new classical T Tauri stars (CTTS) and 66 new weak-line-T Tauri stars (WTTS) with W_{lambda}_(H{alpha})<=10A. Additional pointed ROSAT observations led to the identification of 6 more WTTS and 2 CTTS, giving a total of 76 new T Tauri stars. The large area of our study, as compared with previous works, allows us to study the spatial distribution of WTTS in this star forming region. We find the WTTS of our survey to be distributed over the whole region investigated. There is a noticeable decline of the surface density from south to north within our study area, but the spatial distribution extends most probably beyond our study region. No clustering towards the population of T Tauri stars known prior to ROSAT in Taurus-Auriga could be observed. We suggest that the WTTS found in our study might in part be somewhat older than the previously known T Tauri stars in Taurus-Auriga, and that their broad spatial distribution is due to the typical velocity dispersion of a few km/s measured for Taurus T Tauri stars, in which case for some of our WTTS an age on the order of 10^7^years would be required for reaching the observed distances from the Taurus dark clouds. We estimate a WTTS/CTTS ratio of about 6 within our study area, but conclude that because of the different spatial distribution of WTTS and CTTS this ratio will be most probably significantly larger for a more extended area.
ROSAT
New T Tauri stars in Taurus-Auriga No Number --- Name Identifier of star number=1 HD 285751: this star has independently been detected as T Tauri star by F.M. Walter (1994, private communication); X-ray data are also given in Neuhauser et al. (1995A&A...297..391N) RXJ0458.7+2046 discovered on the basis of preliminary RASS data, but not detected in EXSAS reduction, therefore in table5 for this star no X-ray data are given --- n_Pos Note on position number=2 X : Position is X-ray position, star is not included in Hubble GSC blank : Position is taken from Hubble GSC --- n_Xray Note on X-ray detection number=3 P : Star was discovered by pointed observations blank : Star was discovered by the ROSAT All-Sky Survey --- RAh Right Ascension for equinox 2000.0 h RAm Right Ascension for equinox 2000.0 min RAs Right Ascension for equinox 2000.0 s DEd Declination for equinox 2000.0 deg DEm Declination for equinox 2000.0 arcmin DEs Declination for equinox 2000.0 arcsec EW(Ha) Equivalent width for H_alpha 0.1nm Sp Spectral type --- Pmag Magnitude as listed in the Hubble GSC number=4 For stars not listed in the Hubble GSC a magnitude of 0.0 is given mag Non-TTS emission-line stars found in the course of our survey Name Identifier of star --- n_Pos Note on position number=1 X : Position is X-ray position, star is not included in Hubble GSC blank : Position is taken from Hubble GSC --- n_Xray Note on X-ray detection number=2 P : Star was discovered by pointed observations blank : Star was discovered by the ROSAT All-Sky Survey --- RAh Right Ascension for equinox 2000.0 h RAm Right Ascension for equinox 2000.0 min RAs Right Ascension for equinox 2000.0 s DE- Declination sign --- DEd Declination for equinox 2000.0 deg DEm Declination for equinox 2000.0 arcmin DEs Declination for equinox 2000.0 arcsec CR Background subtracted X-ray count rate (0.1-2.4keV energy range) s-1 e_CR Error in CR s-1 Sp Spectral type --- EW(Ha) Equivalent width for H_alpha 0.1nm ROSAT X-ray data and spectral fit results for new T Tauri stars Name Identifier of star --- n_Pos Note on X-ray data number=1 P : X-ray data are from pointed observations blank : X-ray data are from the ROSAT All-Sky Survey --- ML Maximum likelihood of existence --- Cts Background subtracted X-ray counts (0.1 to 2.4 keV energy range) --- e_Cts Errors for X-ray counts --- Exp Exposure time s HR1 Hardness ratio 1 --- e_HR1 Error in hardness ratio 1 --- HR2 Hardness ratio 2 --- e_HR2 Error in hardness ratio 2 --- log(NH) Logarithm of HI column density number=2 NH and TX are free parameters for the fits of the X-ray spectra cm-2 E_log(NH) Positive error for log(NH) cm-2 e_log(NH) Negative error for log(NH) cm-2 TX Temperature number=2 NH and TX are free parameters for the fits of the X-ray spectra keV E_TX Positive error for TX keV e_TX Negative error for TX keV LX X-ray luminosity (10^30^erg/s) number=3 For the calculation of LX a distance of 140pc has been assumed 10+23W E_LX Positive error for LX 10+23W e_LX Negative error for LX 10+23W X-ray sources in pointed observations Name Identifier of star --- RAh Right Ascension for equinox 2000.0 h RAm Right Ascension for equinox 2000.0 min RAs Right Ascension for equinox 2000.0 s DE- Declination sign --- DEd Declination for equinox 2000.0 deg DEm Declination for equinox 2000.0 arcmin DEs Declination for equinox 2000.0 arcsec Cts Background subtracted X-ray count rate (0.1-2.4 keV energy range) s-1 e_Cts Error in X-ray count rate s-1 HR1 Hardness Ratio 1 --- e_HR1 Error in Hardness Ratio 1 --- HR2 Hardness Ratio 2 --- e_HR2 Error in Hardness Ratio 2 --- table4.tex LaTeX version of table4 table5.tex LaTeX version of table5 table6.tex LaTeX version of table6 table7.tex LaTeX version of table7 figure5a.ps Low-dispersion spectral atlas of new WTTS in Taurus-Auriga. Shown is the H_alpha and Li I region. figure5b.ps Figure5 cont. figure5c.ps Figure5 cont. figure5d.ps Figure5 cont. figure5e.ps Figure5 cont. figure5f.ps Figure5 cont. figure5g.ps Figure5 cont. figure5h.ps Figure5 cont. Patricia Bauer CDS 1996 Apr 10 Rainer Wichmann <R.Wichmann@lsw.uni-heidelberg.de> J_A+A_312_439.xml The redshift-space neighbourhoods of 13 SSRS groups of galaxies J/A+A/312/745 J/A+A/312/745 SSRS groups of galaxies redshift neighbourhood The redshift-space neighbourhoods of 13 SSRS groups of galaxies M Ramella P Focardi M J Geller Astron. Astrophys. 312 745 1996 1996A&A...312..745R Clusters, galaxy Redshifts galaxies: clusters: general galaxies: distances and redshifts galaxies: general The Southern Sky Redshift Survey (SSRS) includes 13 groups of 5 or more members with velocities >=2000km/s. By measuring redshifts and accumulating data from the literature, we increase the total number of known group members from 89 to 218. We also measured new redshifts for 59 foreground/background galaxies superimposed on the group neighborhoods. The velocity dispersions of the groups are remarkably stable.
The groups redshift neighborhood New redshifts in the fore/backgrounds of groups Group Group number (only in table2) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RV Velocity km/s e_RV Mean error on RV km/s Ref Reference for RV number=1 The references are: M = Maia et al. (MdCL), 1989, Ap.J.S. 69,809 =1989ApJS...69..809M 1 = this work, RV from absorption lines in a low resolution spectrum 2 = this work, RV from absorption lines in a high resolution spectrum 3 = this work, RV from absorption lines (average of low and high respective spectrum) 4 = this work, RV from emission lines in a low resolution spectrum 5 = this work, RV from emission lines in a high resolution spectrum 6 = this work, RV from emission lines (average of low and high respective spectrum) --- table2.tex TeX version of table2 table3.tex TeX version of table3 Patricia Bauer CDS 1996 Mar 18 P. Forcadi <pfocardi@astbo4.bo.astro.it> J_A+A_312_745.xml Proper motion study of the globular cluster M92. J/A+A/312/74 J/A+A/312/74 Proper motion of M 92 Proper motion study of the globular cluster M92. H -J Tucholke R -D Scholtz P Brosche Astron. Astrophys. 312 74 1996 1996A&A...312...74T Clusters, globular Proper motions astrometry catalogs Galaxy: kinematics and dynamics globular clusters: individual (M 92) reference systems stars: kinematics We present proper motions for stars in the field of the galactic globular cluster NGC6341 (M92). This study continues the series of papers from the Bonn programme of globular cluster proper motions. Plates taken with the Bonn double refractor and the Rozhen observatory 2m Ritchey-Chretien telescope with a maximal epoch difference of 94 years were used. Relative proper motions for all well-measurable stars in the 1.5degx1.5deg field covered by the plates were derived. Median proper motion errors are 0.8milliarcsec/year (mas/a) for stars brighter than about V=16.7mag. The cluster membership of UV-bright and variable stars is discussed. The proper motions are compared with the accurate relative proper motions of Rees (1992) and with the absolute proper motions from Schmidt plates referred to galaxies of Scholz et al. (1994). The latter comparison enables us to tie the proper motions of the stars and the mean proper motion of M92 to an inertial system. This calibration has an uncertainty of about 1.0mas/a. The absolute proper motions of Hipparcos stars in the field will be useful for the extragalactic calibration of the Hipparcos proper motion system. The data for 642 stars within 18.6' from the cluster centre is available via the CDS (Centre des Donnees Astronomiques Strasbourg) Data Centre.
Proper motion of M 92 RAh Right Ascension J2000, Epoch 1950.0 h DEdeg Declination J2000, Epoch 1950.0 deg X Distance to cluster centre (in RA) arcsec Y Distance to cluster centre (in Dec) arcsec pmRA Proper motion in RA mas/a e_pmRA Error of pmRA mas/a pmDE Proper motion in Dec mas/a e_pmDE Error of pmDE mas/a Prob Probability of Membership to M92 % Npos Number of positions used --- Bmag B Magnitude mag Ident Cross-Identifications number=1 Roman numeral - dash - number(e.g. VIII-12) or lower-case x plus number: Sandage & Walker (1966) ApJ 143, 313 =1966ApJ...143..313S B plus number: Barnard (1931) Publ. Yerkes Obs. no. 6 =1931PYerO...6....1B Bu plus number: Buonanno et al. (1983) A&AS 53, 1 =1983A&AS...53....1B R plus number: Rees (1992) AJ 103, 1573 =1992AJ....103.1573R C plus number: Cudworth (1976) AJ 81, 975 =1976AJ.....81..975C V plus number: Variable star from Sawyer Hogg (1973) Publ. DDO V. 3 no. 6 =1973PDDO....3....6S K plus number: Kadla et al. (1983) Per. Zvezdy 21, 827 =1983PZ.....21..827K N plus number: Nassau (1938) ApJ 87, 361 =1938ApJ....87..361N ZNG plus number : Zinn et al. (1972) A&A 18, 390 =1972A&A....18..390Z S plus number: Sanduleak (1989) ApJS 71, 713 =1989ApJS...71..713S HIC plus number: Hipparcos Input Catalogue, Turon et al. (1992) ESA SP-1136 =Catalogue <I/196> --- Patricia Bauer CDS 1996 Feb 08 H.-J. Tucholke <tucholke@astro.uni-bonn.de> J_A+A_312_74.xml ROSAT survey of stellar X-ray sources in the young open cluster NGC 2516 J/A+A/312/818 J/A+A/312/818 NGC 2516 X-ray sources ROSAT survey of stellar X-ray sources in the young open cluster NGC 2516 J Dachs W Hummel Astron. Astrophys. 312 818 1996 1996A&A...312..818D Clusters, open X-ray sources open clusters and associations: individual (NGC 2516) stars: chemically peculiar stars: coronae stars: emission-line, Be X-rays: stars The ROSAT PSPC detector was used to obtain a deep pointing with its center on the young open cluster NGC 2516 and total integration time of 9284 sec. Altogether 64 X-ray sources were detected showing strong concentration towards the optical cluster centre. This suggests that most of the sources are actually associated with NGC 2516. 42 of these sources could be identified with optical stars in the field of the cluster; after correction for a mean offset between optical and nominal ROSAT positions of about 13", optical star and X-ray source positions are found to agree, on the average, within about 9", while maximum observed positional differences amount to 27". X-ray sources identified with optical cluster stars include HR 3147 (=HD 66194; B2.5IVe), the visually brightest B star in the cluster, three close visual late B-type binaries (h 4027 A,B, h 4031 A,B, and I 1104 A,B) with projected separations ranging between about 4x10^16^cm and 6x10^16^cm, as well as several (six) chemically peculiar Bp/Ap(Si) and Ap(SrCrEu) stars.
ROSAT
X-ray sources detected in NGC 2516 No Running number (increasing with {alpha}) --- Seq X-ray source number, as detected with EXSAS reduction package (increasing with -{delta}) --- m_Seq Multiplicity index on Seq --- RAh Right ascension (2000.0) number=1 The coordinates are corrected for pointing offset of (+1.6s, 4.7") h RAm Right ascension (2000.0) number=1 The coordinates are corrected for pointing offset of (+1.6s, 4.7") min RAs Right ascension (2000.0) number=1 The coordinates are corrected for pointing offset of (+1.6s, 4.7") s DE- Declination sign --- DEd Declination (2000.0) number=1 The coordinates are corrected for pointing offset of (+1.6s, 4.7") deg DEm Declination (2000.0) number=1 The coordinates are corrected for pointing offset of (+1.6s, 4.7") arcmin DEs Declination (2000.0) number=1 The coordinates are corrected for pointing offset of (+1.6s, 4.7") arcsec Dr 90% confidence source radius arcsec u_Dr Undertainty flag on Dr --- CtRate Count rate corrected for vignetting and for the life-time factor (=0.978) ct/s e_CtRate rms uncertainty on Count rate ct/s HR1 Hardness ratio HR1 --- u_HR1 Uncertainty flag on HR1 --- e_HR1 rms uncertainty on HR1 --- HR2 Hardness ration HR2 --- u_HR2 Uncertainty flag on HR2 --- e_HR2 rms uncertainty on HR2 --- Stars in the field of NGC 2516 identified with ROSAT X-ray sources No Running number from table2 --- m_No A ')' indicates the second component of a binary --- Name Identification HD, CPD or CD --- n_Name b = HR 3138; c = HR 3147 --- DK Running number in the photometric study of Dachs and Kabus (1989), hereafter DK --- m_DK Multiplicity index on DK --- Sp Spectral type --- n_Sp A 'g' indicates new spectral type --- RAh Right ascension 2000.0 (optical source) h RAm Right ascension 2000.0 (optical source) min RAs Right ascension 2000.0 (optical source) s n_RA (1) --- DE- Declination sign --- DEd Declination 2000.0 (optical source) deg DEm Declination 2000.0 (optical source) arcmin DEs Declination 2000.0 (optical source) arcsec n_DE (1) --- DRA Position difference ROSAT minus optical in RA number=2 Position difference corrected for pointing offset (+1.6s, -4.7") s n_DRA (1) --- DDE Position difference ROSAT minus optical in DE number=2 Position difference corrected for pointing offset (+1.6s, -4.7") arcsec n_DDE (1) --- Dr Angular distance between optical and X-ray positions arcsec Memb Cluster membership of star, M=member, NM=non-member --- Properties of X-ray sources identified with optical stars of known (or assumed) distance No Running number of table2 --- m_No A ')' indicates the second component of a binary --- Name Identification from table3 HD, CPD, CD or DK --- Sp Spectral type (from DK or this paper) --- Vmag V magnitude (from DK) mag u_Vmag Uncertainty flag on Vmag --- B-V B-V color index (from DK) mag d Adopted distance pc u_d Uncertainty flag on distance --- Mv Inferred absolute visual magnitude mag u_Mv Uncertainty flag on Mv --- Lbol Bolometric luminosity solLum u_Lbol Uncertainty flag on Lbol --- Fx ROSAT X-ray flux (10^-14^erg/cm^2^/s) number=1 Adopted flux conversion factor C_F_ for NGC 2516 cluster stars showing HR1~+1.0: C_F_~1.4x10^-11^erg/cm^2^/s (counts/s)^-1^ 10-14mW/m2 u_Fx Uncertainty flag on Fx --- e_Fx rms uncertainty on Fx 10-14mW/m2 Lx X-ray luminosity (0.16-2.5keV) 10-7W e_Lx Rms uncertainty on Lx 10-7W u_Lx Uncertainty flag on Lx --- -log(Lx/Lbol) -log(X-ray/bolometric luminosities) --- u_-log(Lx/Lbol) Uncertainty flag on -log(Lx/Lbol) --- table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 table6.tex LaTeX version of table6 Patricia Bauer CDS 1996 Apr 16 Wolfgang Hummel <hummel@usm.uni-muenchen.de> J_A+A_312_818.xml Jet-like structures in beta Lyrae. Results of optical interferometry, spectroscopy and photometry J/A+A/312/879 J/A+A/312/879 Beta Lyr radial velocities and UBV data Jet-like structures in beta Lyrae. Results of optical interferometry, spectroscopy and photometry P Harmanec F Morand D Bonneau Y Jiang S Yang E F Guinan D S Hall D Mourard P Hadrava H Bozic C Sterken I Tallon-Bosc G A H Walker G P McCook F Vakili P Stee J M Le Contel Astron. Astrophys. 312 879 1996 1996A&A...312..879H Binaries, eclipsing Radial velocities Photometry, UBV stars: emission-line, Be binaries: eclipsing Stars: individual: beta Lyr techniques: interferometric A preliminary analysis of an extensive collection of interferometric, spectroscopic and photometric observations of the bright Be star {beta} Lyr lead to the following main conclusions: (1) The bulk of the H{alpha} and He I 6678 emission seems to originate in jets of material perpendicular to the orbital plane of the binary. The jets are associated with the more massive component of the binary (star 1) and probably emanate from the `hot spot' in the disk, i.e. the region of interaction of the gas stream flowing from the Roche-lobe filling B6-8II component (star 2) toward star 1. Some contribution to the emission also comes from a region located between the two stars (the gas stream and the `hot spot') and from the `pseudoatmosphere' of the accretion disk around star 1. (2) The 282-d cyclic variation of the light curve of {beta} Lyr is confirmed on the basis of 2852 homogenized V-band observations covering an interval of 36yrs. We find, however, that the amplitude and phase of these variations vary with the orbital phase: the long-term modulation of the light curve almost disappears near orbital phases 0.25P and 0.50P (elongation and secondary eclipse). (3) Pronounced line-profile variations of the H{alpha} and He I 6678 lines on a time scale shorter than one orbital period were clearly detected. They may be periodic, with a period near 4.70-4.75d, and this periodicity may be related to the 282-d change via the orbital period.
Beta Lyr HD 174638 18 50 04.7 +33 21 45.7
Beta Lyr individual radial velocities of the H alpha line (Reticon Ondrejov) Beta Lyr individual radial velocities of the H alpha line (DAO CCD 4096 spectra) No File number --- HJD Heliocentric julian date d cycle Cycle d RVem Radial velocity of emission wings number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVpV Radial velocity of V (violet) peak number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVpR Radial velocity of R (red) peak number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVabs Radial velocity of absorption component number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVstar2 Mean stellar velocity of star2 km/s Beta Lyr individual radial velocities of the He I 6678 line (Reticon Ondrejov) No File number --- HJD Heliocentric julian date d cycle Cycle d RVem Radial velocity of emission wings number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVabs1 Radial vel. of peak main absorption number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVabs2 Radial vel. of peak main absorption number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVabs3 Radial vel. of peak main absorption number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVstar2 Mean stellar velocity of star2 number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVabs4 Radial vel. of other absorption number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVabs5 Radial vel. of other absorption number=1 The value 9999. denotes missing items, no measurements was possible. km/s Beta Lyr individual radial velocities of the He I 6678 line (DAO CCD 4096 spectra) No File number --- HJD Heliocentric julian date d cycle Cycle d RVe Radial velocity of emission wings km/s RVpV Radial velocity of V peak km/s RVpR Radial velocity of R peak km/s RVabs1 Radial velocity of absorption component 1 km/s RVstar2 Mean stellar velocity of star2 number=1 The value 9999. denotes missing items, no measurements was possible. km/s RVabs2 Radial vel. of absorption component 2 number=1 The value 9999. denotes missing items, no measurements was possible. km/s sat.abs Radial vel. of satellite absorption number=1 The value 9999. denotes missing items, no measurements was possible. km/s UBV observations of Beta Lyr, 8 Lyr and 9 Lyr Name Star name --- HJD Heliocentric julian date d w Weight of the observation --- Vmag V magnitude number=1 The value 99.999 denotes missing items, no measurements was possible. Comparison stars used: -------------------------------------------------------------------- HD star V B-V U-B -------------------------------------------------------------------- 172044 HR 6997 5.423 -.094 -.518 176437 Gamma Lyr 3.253 -.071 -.052 174585 8 Lyr 5.929 -.142 -.715 -------------------------------------------------------------------- mag Bmag B magnitude number=1 The value 99.999 denotes missing items, no measurements was possible. Comparison stars used: -------------------------------------------------------------------- HD star V B-V U-B -------------------------------------------------------------------- 172044 HR 6997 5.423 -.094 -.518 176437 Gamma Lyr 3.253 -.071 -.052 174585 8 Lyr 5.929 -.142 -.715 -------------------------------------------------------------------- mag Umag U magnitude number=1 The value 99.999 denotes missing items, no measurements was possible. Comparison stars used: -------------------------------------------------------------------- HD star V B-V U-B -------------------------------------------------------------------- 172044 HR 6997 5.423 -.094 -.518 176437 Gamma Lyr 3.253 -.071 -.052 174585 8 Lyr 5.929 -.142 -.715 -------------------------------------------------------------------- mag B-V B-V color number=1 The value 99.999 denotes missing items, no measurements was possible. Comparison stars used: -------------------------------------------------------------------- HD star V B-V U-B -------------------------------------------------------------------- 172044 HR 6997 5.423 -.094 -.518 176437 Gamma Lyr 3.253 -.071 -.052 174585 8 Lyr 5.929 -.142 -.715 -------------------------------------------------------------------- mag U-B U-B color number=1 The value 99.999 denotes missing items, no measurements was possible. Comparison stars used: -------------------------------------------------------------------- HD star V B-V U-B -------------------------------------------------------------------- 172044 HR 6997 5.423 -.094 -.518 176437 Gamma Lyr 3.253 -.071 -.052 174585 8 Lyr 5.929 -.142 -.715 -------------------------------------------------------------------- mag HDcomp Name of the comparison star --- Site Site (see note4 file) --- Patricia Bauer CDS 1996 Apr 11 Petr Harmanec <hec@sunstel.asu.cas.cz> J_A+A_312_879.xml The systemic-velocity distribution of cataclysmic variables J/A+A/312/93 J/A+A/312/93 Cataclysmic variables systemic-velocity The systemic-velocity distribution of cataclysmic variables J Van Paradijs T Augusteijn R Stehle Astron. Astrophys. 312 93 1996 1996A&A...312...93V V/82 : Cataclysmic binaries (Ritter & Kolb, 1995) Binaries, cataclysmic Radial velocities accretion, accretion disks novae, cataclysmic variables stars: distances stars: kinematics We have collected {gamma} velocities of cataclysmic variables from a survey of published orbital radial-velocity studies. We argue that for the non-magnetic cataclysmic variables the {gamma} distribution gives a fair description of the systemic radial velocities; for magnetic cataclysmic variables the effect of motions within the system appears to be substantial. Assuming that the distribution of the spatial velocities of cataclysmic variables in the solar neighbourhood follows the velocity ellipsoid, with dispersions as given by Wielen (1977), we estimate that the dispersion of z-velocities of CVs is in the range 16 to 21km/s. With the galactic potential of Kuijken and Gilmore (1989) we then derive the distribution of distances, z, above the galactic plane. This distribution has an exponential scale height in the range 160-230pc, which is nearly a factor of two larger than that obtained for the z distribution of systems with known distances. This probably reflects the incompleteness of the census of cataclysmic variables at distances even as small as ~100pc. The velocity distribution of cataclysmic variables indicates that they are an old disk population, with a mix of ages up to 10Gyr.
Radial velocities of cataclysmic variables Name Source name --- Type Type number=1 the types are: AM AM Herculis (subtype cataclysmic variables) DN Dwarf Nova (subtype cataclysmic variables) DQ DQ Herculis (subtype cataclysmic variables) IP Intermediate Polars NA Novae A type NB Novae B type NL Nova like objects SU SU Ursae Majoris (subtype cataclysmic variables) UG U Geminorum (subtype cataclysmic variables) UX UX Ursae Majoris (subtype cataclysmic variables) ZC Z Camelopardalis (subtype cataclysmic variables) For more information see: B. Warner, 'Cataclysmic Variables', Cambridge University Press (1995) or H. Ritter and U. Kolb, in 'X-ray Binaries', Eds W.H.G. Lewin, J. van Paradijs, & E.P.J. van den Heuvel, Cambridge University Press (1995) (catalog <V/82>) --- RV Radial velocity km/s u_RV Uncertainty flag on radial velocity --- Ref Reference codes (see refs file) --- References Ref Reference number --- Text Text of reference --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 Feb 02 J_A+A_312_93.xml Variational principle for slender flux tubes. I. General equations and added mass effects. J/A+A/313/1008 J/A+A/313/1008 Slender flux tubes variational principle . I. Variational principle for slender flux tubes. I. General equations and added mass effects. A Achterberg Astron. Astrophys. 313 1008 1996 1996A&A...313.1008A Magnetic fields Sun magnetic fields MHD Sun: magnetic fields The equation of motion governing slender flux tubes is derived using a variational principle. I consider the interaction between the tube and its surroundings due to buoyancy, added mass (anisotropic inertia) and hydrodynamic drag. It is pointed out that the application of the simple added mass formula commonly used in the litterature is in fact limited to the case of an unstratified, non-rotating flow.
appen.tex LaTeX version of appendix Patricia Bauer CDS 1996 May 23 Bram Achterberg <A.Achterberg@fys.ruu.nl> J_A+A_313_1008.xml Stellar populations and color gradients in the post core collapse globular cluster M30 J/A+A/313/129 J/A+A/313/129 Positions and magnitudes of M30 blue stars Stellar populations and color gradients in the post core collapse globular cluster M30 D Burgarella V Buat Astron. Astrophys. 313 129 1996 1996A&A...313..129B Clusters, globular Stars, blue globular clusters: individual (Messier 30) stars: evolution stars: Population II Sub-arcsec B and V images of the central 2.5arcmin of the post-core-collapse globular cluster M 30 are used to study the stellar populations lying in the central parts of this cluster and to analyze the influence of the stellar content on the radial color gradient reported for this cluster. We find a populated blue horizontal branch which follows a flat radial distribution. The red giants (defined as the objects above the horizontal branch in this paper) are found to be depleted relatively to the other bright detected stellar populations. A highly concentrated population of 42 blue stragglers has also been detected. The presence of a B-V color gradient (0.20-0.24mag/dex) is confirmed. A blueing is detectable from the cluster center out to the edge of the images at r=~1arcmin. None of the detected bright stellar populations (red giant branch, horizontal branch, asymptotic giant branch and blue straggler stars) is found to be at the origin of this gradient. This result suggests that the stellar population(s) responsible for this gradient has still to be identified. Some plausible candidates are tentatively proposed in this paper.
M 30 NGC 7099 C 2137-234 21 40.3 -23 11
Positions and magnitudes of the detected blue horizontal branch stars Positions and magnitudes of the detected blue straggler stars ID Identification number of the star --- Xpos X position relative to our center (see paper) arcsec Ypos Y position relative to our center (see paper) arcsec Rpos Radial distance to our center (see paper) arcsec Vmag V magnitude mag B-V B-V color mag Patricia Bauer CDS 1996 Apr 10 Denis Burgarella <burgarella@lasm0a.astrsp-mrs.fr> J_A+A_313_129.xml Near-infrared and optical broadband surface photometry of 86 face-on disk dominated galaxies. IV. Using color profiles to study stellar and dust content of galaxies. J/A+A/313/377 J/A+A/313/377 Near-IR photometry of 86 galaxies. IV. Near-infrared and optical broadband surface photometry of 86 face-on disk dominated galaxies. IV. Using color profiles to study stellar and dust content of galaxies. R S De Jong Astron. Astrophys. 313 377 1996 1996A&A...313..377D J/A+AS/118/557 : Part II. A two-dimensional method to determine bulge and disk parameters. Galaxies, photometry dust, extinction galaxies: evolution galaxies: fundamental parameters galaxies: photometry galaxies: spiral galaxies: stellar content This Appendix to Paper IV describes the 3D Monte Carlo radiative transfer simulations of dust and stars in exponential disks. The reddening as function of wavelength and as function of radius is used in the main text in a comparison with BVRIHK data of 86 spiral galaxies.
appen.tex LaTex Version of Appendix coorfig2.ps PostScript file of fig.1, coordinate system bivk1.ps PostScript file of fig.2, color-color plots bivk2.ps PostScript file of fig.2 bvrk1.ps PostScript file of fig.2 bvrk2.ps PostScript file of fig.2 Patricia Bauer CDS 1996 Apr 02 Roelof de Jong <R.S.deJong@durham.ac.uk> J_A+A_313_377.xml Evidence for a binary lens in the MACHO LMC No.1 microlensing event J/A+A/313/841 J/A+A/313/841 MACHO LMC No.1 microlensing event Evidence for a binary lens in the MACHO LMC No.1 microlensing event M Dominik A C Hirshfeld Astron. Astrophys. 313 841 1996 1996A&A...313..841D Gravitational lensing dark matter Galaxy: halo gravitational lensing stars: low-mass, brown dwarfs During the last three years, several galactic microlensing events towards the Large Magellanic Cloud and the Galactic Bulge have been detected by four observing groups (MACHO, EROS, OGLE, DUO). Most of these are commonly explained as due to microlensing of a point source by a point mass lens. In this paper, we discuss statistical methods to determine the goodness-of-fit for a specific model of source and lens beyond the assumption that the errors are normal. In particular, we argue that the MACHO LMC#1 event has been caused by a binary lens and thereby confirm our hypothesis (Dominik & Hirshfeld 1994). We also show that the binary lens fit is not unique by presenting alternative plausible binary lens fits. We emphasize that knowledge of the fraction of binaries among the observed microlensing events is crucial for estimating the mass distribution of the observed dark objects. We finally show that for each data set of parameters for a binary source, two physical configurations with different distances between the components exist which produce exactly the same light curve.
appen.tex LaTeX version of appendix A, B and C fig5a.ps PostScript file with Figure 5a fig5b.ps PostScript file with Figure 5b Patricia Bauer CDS 1996 Apr 02 Martin Dominik <dominik@fliewatuet.physik.uni-dortmund.de> J_A+A_313_841.xml Solar chromospheric structures as observed simultaneously in strong UV lines. II. Network and cell modelling. J/A+A/313/949 J/A+A/313/949 Solar chromospheric structures. II. Solar chromospheric structures as observed simultaneously in strong UV lines. II. Network and cell modelling. K Bocchialini P Gouttebroze Astron. Astrophys. 313 949 1996 1996A&A...313..949B Line Profiles Sun lline: profiles Sun: chromosphere Sun: UV radiation Mean line profiles of the quiet Sun spectrum, recorded simultaneously in L{alpha}, L{beta}, Ca II H and K, and Mg II h and k lines with the OSO-8/LPSP spectrometer were derived for structures such as supergranulation cell and network. We compare these observed profiles with theoretical ones computed by Vernazza et al. (1981, VAL81) and by Fontenla et al. (1993, FAL93). We also present our own theoretical profiles : with our non-LTE radiative transfer codes, we compute the line profiles corresponding to different atmospheric models, derived from the reference VAL and FAL models. Finally, we propose two new semi-empirical models, NET and CEL, which are in better agreement with the network and cell line profiles observed by OSO-8.
CEL model (model of a cell structure) NET model (model of a network structure) Mcol Column mass g/cm2 Height Height km T Temperature K Vel Velocity km/s NH Hydrogen density cm-3 Ne Eletron density cm-3 table5.tex LaTeX version of table5 table6.tex LaTeX version of table6 Patricia Bauer CDS 1996 Feb 02 K. Bocchialini <BOCCHIALINI@iasset.ias.fr> UNKNOWN UNKNOWN An inversion between NH and Ne columns was detected by the authors. In the first line of table5, T=100000. instead of 1000000. The correction has been made on 4-Mar-1997 J_A+A_313_949.xml Abundances of light elements in metal-poor stars. I. Atmospheric parameters and a new Teff scale. J/A+A/314/191 J/A+A/314/191 Atmospheric parameters in metal-poor stars. I Abundances of light elements in metal-poor stars. I. Atmospheric parameters and a new Teff scale. R G Gratton E Carretta F Castelli Astron. Astrophys. 314 191 1996 1996A&A...314..191G Abundances Stars, metal-deficient stars: abundances stars: atmospheres stars: fundamental parameters stars: Population II We present atmospheric parameters for about 300 stars of different chemical composition, whose spectra will be used to study the galactic enrichment of Fe and light elements. These parameters were derived using an homogeneous iterative procedure, which considers new calibrations of colour-T_eff_ relations for F, G and K-type stars based on Infrared Flux Method (IRFM) and interferometric diameters for population I stars, and the Kurucz (1992) model atmospheres. We found that these calibrations yield a self-consistent set of atmospheric parameters for T_eff_>4400K, representing a clear improvement over results obtained with older model atmospheres. Using this T_eff_ -scale and Fe equilibrium of ionization, we obtained very low gravities (implying luminosities incompatible with that expected for RGB stars) for metal-poor stars cooler than 4400K; this might be due either to a moderate Fe overionization (expected from statistical equilibrium calculations) or to inadequacy of Kurucz models to describe the atmospheres of very cool giants. Our T_eff_ scale is compared with other scales recently used for metal-poor stars; it agrees well with those obtained using Kurucz (1992) models, but it gives much larger T_eff_'s than those obtained using OSMARCS models (Edvardsson et al. 1993). This difference is attributed to the different treatment of convection in the two sets of models. For the Sun, the Kurucz (1992) model appears to be preferable to the OSMARCS ones because it better predicts the solar limb darkening; furthermore, we find that our photometric T_eff_ 's for metal-poor stars agree well with both direct estimates based on the IRFM, and with T_eff_'s derived from H{alpha} wings when using Kurucz models.
Tables 2,3,4,5 and 6 of the paper Table Number of the table number=1 The table number specifies the sample: 2 = Atmospheric parameters for stars of original sample 3 = Atmospheric parameters for stars of TLLS sample (Tomkin et al., 1992AJ....104.1568T) 4 = Atmospheric parameters for stars of SKPL sample (Sneden et al., 1991AJ....102.2001S) 5 = Atmospheric parameters for stars of E93 sample (Edvardsson et al., 1993A&A...275..101E) 6 = Atmospheric parameters for stars of ZM90 sample (Zhao & Magain, 1990A&A...238..242Z) --- Star Designation --- RAh Right Ascension 2000 (hours) number=2 the positions of the stars have been added at CDS, using the SIMBAD data-base. There is one star ("anon" in Table 4) for which no position could be found. h RAm Right Ascension 2000 (minutes) number=2 the positions of the stars have been added at CDS, using the SIMBAD data-base. There is one star ("anon" in Table 4) for which no position could be found. min RAs Right Ascension 2000 (seconds) number=2 the positions of the stars have been added at CDS, using the SIMBAD data-base. There is one star ("anon" in Table 4) for which no position could be found. s DE- Declination 2000 (sign) number=2 the positions of the stars have been added at CDS, using the SIMBAD data-base. There is one star ("anon" in Table 4) for which no position could be found. --- DEd Declination 2000 (degrees) number=2 the positions of the stars have been added at CDS, using the SIMBAD data-base. There is one star ("anon" in Table 4) for which no position could be found. deg DEm Declination 2000 (minutes) number=2 the positions of the stars have been added at CDS, using the SIMBAD data-base. There is one star ("anon" in Table 4) for which no position could be found. arcmin DEs Declination 2000 (seconds) number=2 the positions of the stars have been added at CDS, using the SIMBAD data-base. There is one star ("anon" in Table 4) for which no position could be found. arcsec Teff Effective Temperature K logg Suface gravity cm/s2 [A/H] Abundance [A/H] (logarithmic scale) Sun Vel Microturbulent velocities km/s Slope Slope of relation between abundances and excitation potential (Only in table2) --- Patricia Bauer, Francois Ochsenbein CDS 1996 Oct 24 R.G. Gratton <gratton@pdmida.pd.astro.it> J_A+A_314_191.xml Predictions of the mutual events of the Galilean satellites of Jupiter occurring in 1997 J/A+A/314/312 J/A+A/314/312 Galilean satellites mutual events in 1997 Predictions of the mutual events of the Galilean satellites of Jupiter occurring in 1997 J -E Arlot Astron. Astrophys. 314 312 1996 1996A&A...314..312A Occultations Planets ephemerides occultations planets and satellites: individual (satellites of Jupiter) This paper provides the predictions of the mutual phenomena of the Galilean satellites which will occur in 1997. Past experiences have shown the interest of the observation of such events very rare, since they occur only every 6 years when the Earth and the Sun pass through the common orbital plane of the Galilean satellites.
*Mutual events: predictions with G-5 ephemeris MaxY Maximum of magnitude drop (year) --- MaxM Maximum of magnitude drop (month) --- MaxD Maximum of magnitude drop (day) --- Event Type of event number=1 1O2 means that J1 will occult J2 3E4 means that J3 will eclipse J4 C means close approach with probably not magnitude drop observable P means partial event A means annular T total nothing is indicated in case of an eclipse by the penumbra --- Maxh Maximum of magnitude drop (hour) h Maxm Maximum of magnitude drop (min) min Maxs Maximum of magnitude drop (sec) s Mag Light flux drop at the time of the minimum of light number=2 1: total desappearance 0: grazing event with probably no detectable magnitude drop Note that the flux drop is calculated referred to the light flux of both involved satellites in case of an occultation and to the light flux of the only eclipsed satellite in case of an eclipse --- Duration Duration of the event s n_Duration [1] Note on duration number=3 1: occultation of J3 by J2 on April 6, 1998. This double event will occur as follows: first contact at 14h 54m 50s, first maximum of the magnitude drop at 15h 39m 0s, increase of the light flux until 17h 21m 0s (the two satellites are than near the external contact but always overlapping), second maximum of the magnitude drop at 19h 25m 18s and final external contact (end of the occultation) at 20h 20m 12s. --- DistJup Distance of the eclipsed or occulted satellite to the center of Jupiter in Jovian radii in order to know the configuration during the observation --- Impact Impact parameter i.e. the minimum distance between the satellites during the event (distance to the shadow cone for eclipse) arcsec tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Sep 04 Jean-Eudes Arlot <Jean-Eudes.Arlot@bdl.fr> J_A+A_314_312.xml Broad emission-line profile variability in NGC 5548. The optical emission lines in 1989. J/A+A/314/43 J/A+A/314/43 NGC 5548 Profile variability Broad emission-line profile variability in NGC 5548. The optical emission lines in 1989. W Kollatschny M Dietrich Astron. Astrophys. 314 43 1996 1996A&A...314...43K Galaxies, Seyfert Line Profiles galaxies: individual (NGC 5548) galaxies: Seyfert line: profiles Optical emission line intensities of the variable Seyfert 1 galaxy NGC 5548 are presented.
NGC 5548 14 17 59.5 +25 08 13
*Integrated emission-line intensities of the intercalibrated spectra HJD Heliocentric Julian date d Halpha Halpha {lambda}6563 line flux 10-13mW/m2 e_Halpha rms uncertainty on Halpha 10-13mW/m2 Hbeta Hbeta {lambda}4861 line flux 10-13mW/m2 e_Hbeta rms uncertainty on Hbeta 10-13mW/m2 Hgamma Hgamma {lambda}4340 line flux 10-13mW/m2 e_Hgamma rms uncertainty on Hgamma 10-13mW/m2 HeI HeI {lambda}5876 line flux 10-13mW/m2 e_HeI rms uncertainty on HeI 10-13mW/m2 HeII HeII {lambda}4686 line flux 10-13mW/m2 e_HeII rms uncertainty on HeII 10-13mW/m2 table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 May 24 W. Kollatschny <wkollat@gwdg.de> J_A+A_314_43.xml An analysis of the Ap spectroscopic binary HD 59435 J/A+A/314/491 J/A+A/314/491 HD 59435 radial velocity & Geneva photometry An analysis of the Ap spectroscopic binary HD 59435 G Wade P North G Mathys S Hubrig Astron. Astrophys. 314 491 1996 1996A&A...314..491W Photometry, Geneva Radial velocities Stars, Ap binaries: spectroscopic stars: chemically peculiar stars: evolution stars: individual (HD 59435) stars: magnetic fields Radial velocities obtained with the Coravel scanner and with the ESO CES spectrograph are combined with Teff estimates and theoretical evolutionary tracks to determine the masses and luminosities of both components of the SB2 binary HD 59435. The surface magnetic field of the Ap secondary is measured from high resolution CES spectra. For a general description of the Geneva photometric system, see e.g. <GCPD/13>
HD 59435 07 29 35.41 -09 15 33.8
CORAVEL radial velocities of HD 59435 CES spectra radial velocities of HD 59435 HJD1 Heliocentric Julian date of observation of the Primary (cooler) component d RV1 Radial velocity of the primary component km/s e_RV1 rms uncertainty on RV1 km/s HJD2 Heliocentric Julian date of observation of the secondary (hotter) component d RV2 Radial velocity of the secondary component km/s e_RV2 rms uncertainty on RV2 km/s Visual magnitudes and colour indices of HD 59435 in the Geneva photometric system HJD Heliocentric Julian day d Q Photometric Q weight (Rufener 1988) --- Vmag Magnitude in the visible mag P Photometric P weight (Rufener 1988) --- [U-B] Geneva [U-B] index mag [V-B] Geneva [V-B] index mag [B1-B] Geneva [B1-B] index mag [B2-B] Geneva [B2-B] index mag [V1-B] Geneva [V1-B] index mag [G-B] Geneva [G-B] index mag tables.tex LaTeX version of table1 & table2 Patricia Bauer CDS 1996 May 03 Pierre North <north@scsun.unige.ch> J_A+A_314_491.xml Search for resonance effects in long period Cepheids J/A+A/314/541 J/A+A/314/541 Long period Cepheids Search for resonance effects in long period Cepheids E Antonello P L Morelli Astron. Astrophys. 314 541 1996 1996A&A...314..541A Stars, variable Cepheids stars: oscillations The light curves of 124 classical Cepheids with period longer than 8 days were Fourier decomposed with the aim of detecting resonance effects between pulsation modes in the Fourier parameters.
List of Cepheids RAh Right Ascension 2000 (hours) number=1 Coordinates added at CDS. h RAm Right Ascension 2000 (minutes) number=1 Coordinates added at CDS. min RAs Right Ascension 2000 (seconds) number=1 Coordinates added at CDS. s DE- Declination 2000 (sign) number=1 Coordinates added at CDS. --- DEd Declination 2000 (degrees) number=1 Coordinates added at CDS. deg DEm Declination 2000 (minutes) number=1 Coordinates added at CDS. arcmin Name Star name --- P Period d N Data points --- Order Order of Fourier fit --- sigma Standard deviation of the fit mag Ref References number=2 B: Berdnikov (1986-1995) C: Coulson and Caldwell (1985SAAOC...9....5C) D: Dean et al. (1977MmRAS..83...69D) G: Coulson et al. (1985ApJS...57..595C) M: Madore (1975ApJS...29..219M) MB: Moffett and Barnes (1980ApJS...44..427M, 1984ApJS...55..389M) P: Pel (1976A&AS...24..413P) T: Mitchell et al. (1964BOTT....3..153M) W: Walraven et al. (1965BAN....17..520W) --- Fourier parameters P Period d phi21 Phase difference phi_21 rad phi31 Phase difference phi_31 rad phi41 Phase difference phi_41 rad phi51 Phase difference phi_51 rad phi61 Phase difference phi_61 rad phi71 Phase difference phi_71 rad phi81 Phase difference phi_81 rad R21 Amplitude ratio R2/1 --- R31 Amplitude ratio R3/1 --- R41 Amplitude ratio R4/1 --- R51 Amplitude ratio R5/1 --- R61 Amplitude ratio R6/1 --- R71 Amplitude ratio R7/1 --- R81 Amplitude ratio R8/1 --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Apr 17 Elio Antonello <elio@merate.mi.astro.it> J_A+A_314_541.xml NaI/KI scattering observations in circumstellar envelopes: constraints on ionization and mass-loss rates. J/A+A/314/585 J/A+A/314/585 NaI/KI scattering in circumstellar envelopes NaI/KI scattering observations in circumstellar envelopes: constraints on ionization and mass-loss rates. C Guilain N Mauron Astron. Astrophys. 314 585 1996 1996A&A...314..585G Mass loss Stars, atmospheres circumstellar matter stars: AGB and post-AGB stars: individual (W Hya, R Hya) stars: mass-loss We investigate KI or NaI fluorescent emission in circumstellar shells to study their ionization and mass-loss rates. First-time KI detections around the mira-type stars W Hya and R Hya are presented. Together with the previously analysed cases of {alpha} Ori, {alpha} Her and o Cet (Mauron and Caux 1992) and other observations, this gives an extended sample of 10 envelopes which includes {mu} Ce p, CE Tau, {beta} Peg, {rho} Per and g Her. A few non-detections are also considered. In order to compare observed with expected values of KI intensities, the ionization model of Glassgold and Huggins (1986) is used, and the relevant parameters such as distance d, mass-loss rate {dot}(M), gas temperature, fractional electron abundance x_e_ and stellar photoionizing rates G_{oplus} _have to be known. Using data found in the literature, we estimate these parameters in detail for each case. The values of x_e_ are obtained with a hypothesized simple rule based on the circumstellar abundance of molecules and grains which could lock electron donors, giving either x_e_~3x10^-4^ or ~2x10^-5^. The G_{oplus} _values depend on the rare ultraviolet spectrophotometric data available for red giants. The kinetic temperature was assumed to be 30K at the probed impact parameters r_obs_~0.5 to 5x10^16^cm. Despite real uncertainties, the predicted KI intensities with our best estimates of the parameters are in very reasonable agreement with observations in 8 cases in 10. The largest discrepancy concerns the red supergiant {mu} Cep (M2Ia): our KI data suggest that, similar to {alpha} Ori, CO and dust are incompletely formed; for this object we favor {dot}(M)=5x10^-6^M_{sun}_/yr. The wind of {beta} Peg is the second case for which a larger mass-loss and/or a larger x_e_ than primarily believed is suggested, but confirming observations are needed. Finally there is no indication that K or Na might be depleted in silicate grains.
appen.tex LaTeX version of appendix Patricia Bauer CDS 1996 Sep 19 Nicolas Mauron <mauron@graal.univ-montp2.fr> J_A+A_314_585.xml Maps of the 36 GHz methanol emission J/A+A/314/615 J/A+A/314/615 Maps of the 36 GHz methanol emission Maps of the 36 GHz methanol emission S Liechti T L Wilson Astron. Astrophys. 314 615 1996 1996A&A...314..615L Masers HII regions ISM: clouds ISM: molecules radio lines: ISM We have used the Effelsberg 100-meter telescope to map the 36GHz 4_-1_->3_0_E methanol transition in galactic star forming regions where methanol masers were previously detected. In most sources, the emission consists in one or several narrow (maser) features superimposed on a broader, presumably quasi-thermal component. The line shapes and positions of the narrow features are often similar to those observed in the other ClassI methanol maser transitions (at 25, 44, 84 and 95GHz), but with some exceptions. Our observations confirm that, unlike the strong ClassII methanol masers (at 12.2, and 6.6GHz), the ClassI methanol masers are offset from the compact HII regions, infrared sources and OH/H_2_O masers. In outflow sources, these are located at the edge of the molecular lobes.
Line parameters for detected sources Name Source name number=1 The source name and coordinates are repeated for each detected feature. The sources are ordered in increasing right ascension. --- RAh Right ascension 1950 (hours) number=1 The source name and coordinates are repeated for each detected feature. The sources are ordered in increasing right ascension. h RAm Right ascension 1950 (minutes) number=1 The source name and coordinates are repeated for each detected feature. The sources are ordered in increasing right ascension. min RAs Right ascension 1950 (seconds) number=1 The source name and coordinates are repeated for each detected feature. The sources are ordered in increasing right ascension. s DE- Declination sign --- DEd Declination 1950 (degrees) number=1 The source name and coordinates are repeated for each detected feature. The sources are ordered in increasing right ascension. deg DEm Declination 1950 (arcminutes) number=1 The source name and coordinates are repeated for each detected feature. The sources are ordered in increasing right ascension. arcmin DEs Declination 1950 (arcseconds) number=1 The source name and coordinates are repeated for each detected feature. The sources are ordered in increasing right ascension. arcsec S Integrated flux density of the feature number=2 The integrated flux density (determined from spectral gaussian fit of the feature) is the one at the peak position (see note (3)). If no peak position was determined, it is the maximum integrated area of the different observed positions. Jy.km/s e_S 1 sigma uncertainty on integrated flux Jy.km/s V Center velocity of the feature number=3 The velocity (with respect to the l.s.r.) and width is the mean over the all the observed positions and the 1 sigma uncertainty is the statistical error of this mean. km/s e_V 1 sigma uncertainty on center velocity km/s W Width of the feature number=3 The velocity (with respect to the l.s.r.) and width is the mean over the all the observed positions and the 1 sigma uncertainty is the statistical error of this mean. km/s e_W 1 sigma uncertainty on width km/s dRA R.A. position offset of the feature number=4 The offset is with respect to the R.A. and Dec. position of the source.The position of the emission peak of the feature has been determined by a spatial 2-dimension gaussian fit on the integrated area of the line. The error is the error of the fit and does not include pointing errors. When no fit was performed (line too weak, extended or on the edge of the map), the position given is the position where the maximum flux density has been detected. arcsec e_dRA 1 sigma uncertainty on R.A. position offset arcsec dDE Dec. position offset of the feature number=4 The offset is with respect to the R.A. and Dec. position of the source.The position of the emission peak of the feature has been determined by a spatial 2-dimension gaussian fit on the integrated area of the line. The error is the error of the fit and does not include pointing errors. When no fit was performed (line too weak, extended or on the edge of the map), the position given is the position where the maximum flux density has been detected. arcsec e_dDE 1 sigma uncertainty on dec. position offset arcsec theta Angular size of the feature number=5 Theta is the mean size of the source assuming a gaussian shape, calculated from the mean of the minor and major axis half power width of the elliptical 2-dimensional gaussian fitted on the line area contour map (assuming a 26" HPBW for the telescope beam). Theta is not given when the peak of the detected emission is on the edge of the map, or when the 2-dimension gaussian fit was not performed (2 peaks, too extended, line too weak, ...). arcsec e_theta 1 sigma uncertainty on angular size arcsec Rem Remarks number=6 P: point-like source in our beam (i.e. < 10") td: tentative detection em: peak of the detected emission on the edge of the observed map ex: extended emission uncomp: map uncomplete mf: many features, only the strongest are given --- F-name Other name for the position of the feature --- Non detected sources Name Source name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Vcen Center velocity of observation km/s rms 1 sigma upper limit (spectrum r.m.s. noise) Jy Main detected features in Sgr B2 Main detected features in Sgr A-A Fpeak Peak flux density of the feature Jy Vcen Center velocity of the feature km/s e_Vcen 1 sigma uncertainty on center velocity km/s Width Width of the feature km/s e_Width 1 sigma uncertainty on width km/s dRA Feature right ascension position offset number=1 The offsets are with respect to the position given in Table 1 for Sgr B2 (Table 3) and Sgr A-A (Table 4). arcsec dDE Feature declination position offset number=1 The offsets are with respect to the position given in Table 1 for Sgr B2 (Table 3) and Sgr A-A (Table 4). arcsec table1.tex LaTeX version of table1 figure1.ps Postscript file of figure 1 (with caption) figure3.ps Postscript file of figure 3 (with caption) figure5.ps Postscript file of figure 5 (with caption) figure7.ps Postscript file of figure 7 (with caption) figure8.ps Postscript file of figure 8 (with caption) figure9.ps Postscript file of figure 9 (with caption) figure10.ps Postscript file of figure 10 (with caption) figure11.ps Postscript file of figure 11 (with caption) Patricia Bauer CDS 1996 Apr 16 Stella Liechti <liechti@cay.es> J_A+A_314_615.xml Spectroscopic and speckle interferometric orbit of Gliese 692.1 J/A+A/314/846 J/A+A/314/846 Radial velocities of Gliese 692.1 Spectroscopic and speckle interferometric orbit of Gliese 692.1 A Duquennoy A A Tokovinin C Leinert A Glindemann J -L Halbwachs M Mayor Astron. Astrophys. 314 846 1996 1996A&A...314..846D Radial velocities binaries: spectroscopic binaries: visual stars: individual (HD 161198, Gliese 692.1) The combined spectroscopic and interferometric orbit of the single-lined binary dwarf HD 161198=Gliese 692.1 is derived from the radial velocities measured with two correlation radial-velocity spectrometers, CORAVEL and RVM, and from speckle-interferometry in the near IR. The orbital period is 7.0 years, eccentricity e=0.936. Secondary mass is about 0.3 solar mass.
HD 161198 Gliese 692.1 17 43 16 +21 37 04
Radial velocities and residuals. I. CORAVEL data Radial velocities and residuals. II. RVM data (correction +0.20km/s) HJD Heliocentric Julian date d RV Radial velocity km/s e_RV rms uncertainty on radial velocity km/s DRV Observed minus calculated radial velocities km/s Patricia Bauer CDS 1996 Apr 24 Elisabeth Teichmann <Elisabeth.Teichmann@obs.unige.ch> J_A+A_314_846.xml V Hydrae : the missing link between spherical red giants and bipolar planetary nebulae? Radio observations of the molecular envelope. J/A+A/314/871 J/A+A/314/871 V Hydrae V Hydrae : the missing link between spherical red giants and bipolar planetary nebulae? Radio observations of the molecular envelope. C Kahane P Audinos C Barnbaum M Morris Astron. Astrophys. 314 871 1996 1996A&A...314..871K Stars, giant circumstellar matter radio lines: stars stars: AGB and post-AGB stars: individual (V Hya) stars: mass-loss We have performed fully sampled mapping of CO (J=1-0) and (J=2-1) emission around the red giant carbon star V Hya, with the IRAM 30m telescope. The velocity structure of the lines reveals two symmetric high velocity wings that we interpret as arising from a bipolar flow. Exactly between the red and the blue cones lies a low velocity component showing the same symmetry axis. We suggest that this component is a moderately oblate spheroid with biconical holes centered on the minor axis, or a thick torus with the same symmetry axis as the bipolar flow. The high signal-to-noise ratio and spectral resolution of the data allow a detailed comparison of the observed lines with a model of the envelope. Using this model, we derive the geometrical and kinematical parameters of the bipolar flow: it appears to have a wide opening angle (65deg) and shows a radially decreasing velocity law, starting at a velocity of at least 50km/s at the flow inner radius. We suggest that this behaviour is due to an increase with time of the flow ejection velocity close to the star. In contrast, the low-velocity component expands at a constant velocity of 7.5km/s. From our model we also derive the total mass loss rate of V Hya (~1.5x10^-6^M_{sun}_/yr), with about 90% of the molecular gas expelled in the high-velocity jet. The circumstellar envelope around V Hya contains ~2.1x10^-3^M_{sun}_, with about four times more gas in the bipolar flow than the low-velocity component. We compare our observations with other evidence for asymmetric mass loss from V Hya. Considering also the star's fast rotation revealed by the photospheric lines, we conclude that V Hya is probably experiencing the short binary common envelope evolution phase between the AGB and the planetary nebula stage, where highly asymmetric mass loss develops.
V Hya 10 51 37.27 -21 15 01.1
vhyafig1.ps *PostScript file of fig1 Comparison of two methods used to recenter the individual maps. The black squares on the spectral maps correspond to the same position in the envelope, according to a visual comparison of the line shapes of both maps. It means that the (0,0) position of the map No 5 is shifted by +5arcsec in declination compared to the (0,0) position of the map No 9. The contours represent the intensity in the blue peak of the lines for each map. The dotted lines indicate the maximum of each map. To make the maxima coincide, map No 5 must be shifted by -0.75arcsec in right ascension and +4.75arcsec in declination. vhyafig2.ps *PostScript file of fig2 12CO(2-1) emission towards the circumstellar envelope of V Hya. Due to the shift-and-add technique used to reduce the data, the exact coordinates of the (0,0) position of the map are uncertain but should be close to the coordinates of the star: alpha(1950)=10h49m11.3s, delta(1950)=-20:59:05.0. Linear baselines have been subtracted from the spectra. The velocity resolution is 1.3km/s. vhyafig3.ps *PostScript file of fig3 The same as Fig. 2 for the 12CO(1-0) emission. The velocity resolution is 1.6km/s. Patricia Bauer CDS 1996 May 03 Claudine Kahane <kahane@gag.observ-gr.fr> J_A+A_314_871.xml Optical and infrared observations of 27 oxygen-rich stars. Modelling of the circumstellar dust shells. J/A+A/314/896 J/A+A/314/896 IR fluxes and photometry of oxygen-rich stars Optical and infrared observations of 27 oxygen-rich stars. Modelling of the circumstellar dust shells. P Le Sidaner T Le Bertre Astron. Astrophys. 314 896 1996 1996A&A...314..896L Photometry, UBVRI Stars, giant circumstellar matter infrared: stars radiative transfer radio continuum: stars stars: AGB and post-AGB stars: mass-loss We present mid-infrared (10-20{mu}m) photometry obtained on 27 variable oxygen-rich late-type stars, at different epochs during the period 1984-1990. The sample includes representative objects of Miras with optical counterparts, as well as type II OH/IR sources; there are also at least 2 supergiants. These measurements are merged with near-infrared ones, already reported and obtained quasi-simultaneously, to derive 72 (1-20{mu}m) broad band energy distributions. These results are complemented also with IRAS data and flux measurements obtained in the sub-millimeter range. The resulting spectra are interpreted in terms of a circumstellar dust shell radiative transfer model applied for each object at different phases of their lightcurves. The modelling appears to be consistent for a large variety of oxygen-rich sources with optical depth at 10{mu}m ranging from ~0.01 to 10. The temperature of formation of the grains is taken to range from 800 to 950K depending on the pressure at the site of dust formation (P~10^-7^-10^-4^dyn.cm^-2^). Physical parameters such as inner radius of the circumstellar dust shell, bolometric luminosity and mass-loss rate are evaluated. For the objects in the sample, the mass-loss rate ranges from 2x10^-8^ to 10^-4^M_{sun}_/yr. In the context of the planned and underway near-infrared surveys we discuss the relations between color indices and optical depth for oxygen-rich sources. Circumstellar shell optical depths and mass-loss rates are shown to be correlated to the [K-12{mu}m] color. Unfortunately, near-infrared data alone seem to be insufficient to determine physical parameters reliably. For a description of the UBVRI photometric systems, see e.g. <GCPD/08>
Spectral types and molecular data Name Star name --- IRAS IRAS name --- T IRAS color temperature K Sp Spectral type (the reference number is in ()) number=1 (1) Whitelock et al. (1994MNRAS.267..711W) (2) Caswell et al. (1981AuJPh..34..333C) (3) Haikala (1990A&AS...85..875H) (4) Le Bertre (1993A&AS...97..729L) (5) Comoreto et al. (1990A&AS...84..179C) (6) Alcolea & Bujarrabal (1992A&A...253..475A) (7) Wilson & Barrett (1972A&A....17..385W) (8) Nyman et al. (1992A&AS...93..121N) (9) average of Colomer et al. (1992A&A...254L..17C) (10) Bowers et al. (1993AJ....105..284B) (11) Bowers et al. (1989ApJ...340..479B) (12) Bujarrabal et al. (1989A&A...219..256B) (13) Le Bertre & Nyman (1990A&A...233..477L) (14) Sivagnanam et al. (1989A&A...211..341S) (15) Engels (1979A&AS...36..337E) (16) Deguchi et al. (1989MNRAS.239..825D) (17) te Lintel Hekkert et al. (1991A&AS...90..327T) (18) Nyman et al. (1993A&A...280..551N) (19) Allen et al. (1977ApJ...217..108A) (20) Spencer et al. (1977AJ.....82..706S) (21) Lewis & Engels (1988Natur.332...49L) (22) Eder et al. (1988ApJS...66..183E) (23) Jewell et al. (1991A&A...242..211J) (24) Heske et al. (1990A&A...239..173H) (25) Ivison et al. (1994MNRAS.269..218I) (26) Knapp (1985ApJ...293..273K) (27) Allen et al. (1993ApJ...411..188A) (28) Hansen & Blanco (1975AJ.....80.1011H) (29) Le Bertre & Epchtein (1987A&A...171..116L) (30) Le Bertre (1991A&A...250..351L) --- VSiO SiO velocity km/s n_VSiO Note number=2 nd: not detected; *: velocity of the single peak at 1665 MHz; sp: single peak --- r_VSiO Reference number=1 (1) Whitelock et al. (1994MNRAS.267..711W) (2) Caswell et al. (1981AuJPh..34..333C) (3) Haikala (1990A&AS...85..875H) (4) Le Bertre (1993A&AS...97..729L) (5) Comoreto et al. (1990A&AS...84..179C) (6) Alcolea & Bujarrabal (1992A&A...253..475A) (7) Wilson & Barrett (1972A&A....17..385W) (8) Nyman et al. (1992A&AS...93..121N) (9) average of Colomer et al. (1992A&A...254L..17C) (10) Bowers et al. (1993AJ....105..284B) (11) Bowers et al. (1989ApJ...340..479B) (12) Bujarrabal et al. (1989A&A...219..256B) (13) Le Bertre & Nyman (1990A&A...233..477L) (14) Sivagnanam et al. (1989A&A...211..341S) (15) Engels (1979A&AS...36..337E) (16) Deguchi et al. (1989MNRAS.239..825D) (17) te Lintel Hekkert et al. (1991A&AS...90..327T) (18) Nyman et al. (1993A&A...280..551N) (19) Allen et al. (1977ApJ...217..108A) (20) Spencer et al. (1977AJ.....82..706S) (21) Lewis & Engels (1988Natur.332...49L) (22) Eder et al. (1988ApJS...66..183E) (23) Jewell et al. (1991A&A...242..211J) (24) Heske et al. (1990A&A...239..173H) (25) Ivison et al. (1994MNRAS.269..218I) (26) Knapp (1985ApJ...293..273K) (27) Allen et al. (1993ApJ...411..188A) (28) Hansen & Blanco (1975AJ.....80.1011H) (29) Le Bertre & Epchtein (1987A&A...171..116L) (30) Le Bertre (1991A&A...250..351L) --- VH2O H2O central velocity km/s n_VH2O Note number=2 nd: not detected; *: velocity of the single peak at 1665 MHz; sp: single peak --- r_VH2O Reference number=1 (1) Whitelock et al. (1994MNRAS.267..711W) (2) Caswell et al. (1981AuJPh..34..333C) (3) Haikala (1990A&AS...85..875H) (4) Le Bertre (1993A&AS...97..729L) (5) Comoreto et al. (1990A&AS...84..179C) (6) Alcolea & Bujarrabal (1992A&A...253..475A) (7) Wilson & Barrett (1972A&A....17..385W) (8) Nyman et al. (1992A&AS...93..121N) (9) average of Colomer et al. (1992A&A...254L..17C) (10) Bowers et al. (1993AJ....105..284B) (11) Bowers et al. (1989ApJ...340..479B) (12) Bujarrabal et al. (1989A&A...219..256B) (13) Le Bertre & Nyman (1990A&A...233..477L) (14) Sivagnanam et al. (1989A&A...211..341S) (15) Engels (1979A&AS...36..337E) (16) Deguchi et al. (1989MNRAS.239..825D) (17) te Lintel Hekkert et al. (1991A&AS...90..327T) (18) Nyman et al. (1993A&A...280..551N) (19) Allen et al. (1977ApJ...217..108A) (20) Spencer et al. (1977AJ.....82..706S) (21) Lewis & Engels (1988Natur.332...49L) (22) Eder et al. (1988ApJS...66..183E) (23) Jewell et al. (1991A&A...242..211J) (24) Heske et al. (1990A&A...239..173H) (25) Ivison et al. (1994MNRAS.269..218I) (26) Knapp (1985ApJ...293..273K) (27) Allen et al. (1993ApJ...411..188A) (28) Hansen & Blanco (1975AJ.....80.1011H) (29) Le Bertre & Epchtein (1987A&A...171..116L) (30) Le Bertre (1991A&A...250..351L) --- VOH OH central velocity km/s n_VOH Note number=2 nd: not detected; *: velocity of the single peak at 1665 MHz; sp: single peak --- r_VOH Reference number=1 (1) Whitelock et al. (1994MNRAS.267..711W) (2) Caswell et al. (1981AuJPh..34..333C) (3) Haikala (1990A&AS...85..875H) (4) Le Bertre (1993A&AS...97..729L) (5) Comoreto et al. (1990A&AS...84..179C) (6) Alcolea & Bujarrabal (1992A&A...253..475A) (7) Wilson & Barrett (1972A&A....17..385W) (8) Nyman et al. (1992A&AS...93..121N) (9) average of Colomer et al. (1992A&A...254L..17C) (10) Bowers et al. (1993AJ....105..284B) (11) Bowers et al. (1989ApJ...340..479B) (12) Bujarrabal et al. (1989A&A...219..256B) (13) Le Bertre & Nyman (1990A&A...233..477L) (14) Sivagnanam et al. (1989A&A...211..341S) (15) Engels (1979A&AS...36..337E) (16) Deguchi et al. (1989MNRAS.239..825D) (17) te Lintel Hekkert et al. (1991A&AS...90..327T) (18) Nyman et al. (1993A&A...280..551N) (19) Allen et al. (1977ApJ...217..108A) (20) Spencer et al. (1977AJ.....82..706S) (21) Lewis & Engels (1988Natur.332...49L) (22) Eder et al. (1988ApJS...66..183E) (23) Jewell et al. (1991A&A...242..211J) (24) Heske et al. (1990A&A...239..173H) (25) Ivison et al. (1994MNRAS.269..218I) (26) Knapp (1985ApJ...293..273K) (27) Allen et al. (1993ApJ...411..188A) (28) Hansen & Blanco (1975AJ.....80.1011H) (29) Le Bertre & Epchtein (1987A&A...171..116L) (30) Le Bertre (1991A&A...250..351L) --- VexpOH OH expansion velocity km/s VCO CO central velocity km/s n_VCO Note number=2 nd: not detected; *: velocity of the single peak at 1665 MHz; sp: single peak --- r_VCO Reference number=1 (1) Whitelock et al. (1994MNRAS.267..711W) (2) Caswell et al. (1981AuJPh..34..333C) (3) Haikala (1990A&AS...85..875H) (4) Le Bertre (1993A&AS...97..729L) (5) Comoreto et al. (1990A&AS...84..179C) (6) Alcolea & Bujarrabal (1992A&A...253..475A) (7) Wilson & Barrett (1972A&A....17..385W) (8) Nyman et al. (1992A&AS...93..121N) (9) average of Colomer et al. (1992A&A...254L..17C) (10) Bowers et al. (1993AJ....105..284B) (11) Bowers et al. (1989ApJ...340..479B) (12) Bujarrabal et al. (1989A&A...219..256B) (13) Le Bertre & Nyman (1990A&A...233..477L) (14) Sivagnanam et al. (1989A&A...211..341S) (15) Engels (1979A&AS...36..337E) (16) Deguchi et al. (1989MNRAS.239..825D) (17) te Lintel Hekkert et al. (1991A&AS...90..327T) (18) Nyman et al. (1993A&A...280..551N) (19) Allen et al. (1977ApJ...217..108A) (20) Spencer et al. (1977AJ.....82..706S) (21) Lewis & Engels (1988Natur.332...49L) (22) Eder et al. (1988ApJS...66..183E) (23) Jewell et al. (1991A&A...242..211J) (24) Heske et al. (1990A&A...239..173H) (25) Ivison et al. (1994MNRAS.269..218I) (26) Knapp (1985ApJ...293..273K) (27) Allen et al. (1993ApJ...411..188A) (28) Hansen & Blanco (1975AJ.....80.1011H) (29) Le Bertre & Epchtein (1987A&A...171..116L) (30) Le Bertre (1991A&A...250..351L) --- VexpCO CO expansion velocity km/s 10-20 microns photometric data Name Star name --- Date Heliocentric Julian Date d Nmag N magnitude (10.36 microns) mag N1mag N1 magnitude (8.38 microns) mag N2mag N2 magnitude (9.69 microns) mag N3mag N3 magnitude (12.89 microns) mag Q0mag Q0 magnitude (18.06 microns) mag 0.36-0.80 microns photometric data Name Star name --- HJD Heliocentric Julian date d Umag U magnitude mag Bmag B magnitude mag Vmag V magnitude mag Rmag R magnitude mag Imag I magnitude mag Sub-millimeter continuum fluxes Name Star name --- l_S400 Limit flag on S400 --- S400 Flux at 400 {mu}m Jy r_S400 Reference for S400 number=1 (1) Sopka et al. (1985ApJ...294..242S) (2) Marshall et al. (1992PASP..104..397M) (3) Wamsley et al. (1991A&A...248..555W) (4) van der Veen et al. (1995A&A...295..445V) --- W400 400{mu}m beam width Jy S450 Flux at 450{mu}m Jy r_S450 Reference for S450 number=1 (1) Sopka et al. (1985ApJ...294..242S) (2) Marshall et al. (1992PASP..104..397M) (3) Wamsley et al. (1991A&A...248..555W) (4) van der Veen et al. (1995A&A...295..445V) --- W450 450{mu}m beam width Jy S800 Flux at 800{mu}m Jy r_S800 Reference for S800 number=1 (1) Sopka et al. (1985ApJ...294..242S) (2) Marshall et al. (1992PASP..104..397M) (3) Wamsley et al. (1991A&A...248..555W) (4) van der Veen et al. (1995A&A...295..445V) --- W800 800{mu}m beam width Jy S1.1 Flux at 1.1mm mJy r_S1.1 Reference for S1.1 --- W1.1 1.1mm beam width mJy S1.3 Flux at 1.3mm mJy r_S1.3 Reference for S1.3 number=1 (1) Sopka et al. (1985ApJ...294..242S) (2) Marshall et al. (1992PASP..104..397M) (3) Wamsley et al. (1991A&A...248..555W) (4) van der Veen et al. (1995A&A...295..445V) --- W1.3 1.3mm beam width mJy Comparison of IRAS fluxes and model predictions Model Grain model 1: Jones and Merrill (1976) 2: table8 --- Name Star name --- Phase Phase of the variable star --- IRAS60 IRAS flux at 60{mu}m Jy S60,0,T Model 60{mu}m flux for an interstellar density of 0 H atom/cm^3 Jy S60,0,P Model 60{mu}m flux for ID=0 H atom/cm^3, measured within a beam of 3.15 arcmin Jy S60,1,T Model 60{mu}m flux for an interstellar density of 1 H atom/cm^3 Jy S60,1,P Model 60{mu}m flux for ID=1 H atom/cm^3, measured within a beam of 3.15 arcmin Jy S60,10,T Model 60{mu}m flux for an interstellar density of 10 H atom/cm^3 Jy S60,10,P Model 60{mu}m flux for ID=10 H atom/cm^3, measured within a beam of 3.15 arcmin Jy l_IRAS100 limit flag on IRAS100 --- IRAS100 IRAS flux at 100{mu}m Jy S100,0,T Model 100{mu}m flux for an interstellar density of 0 H atom/cm^3 Jy S100,0,P Model 100{mu}m flux for ID=0 H atom/cm^3, measured within a beam of 4.25 arcmin Jy S100,1,T Model 100{mu}m flux for an interstellar density of 1 H atom/cm^3 Jy S100,1,P Model 100{mu}m flux for ID=1 H atom/cm^3, measured within a beam of 4.25 arcmin Jy S100,10,T Model 100{mu}m flux for an interstellar density of 10 H atom/cm^3 Jy S100,10,P Model 100{mu}m flux for ID=10 H atom/cm^3, measured within a beam of 4.25 arcmin Jy S200,0,T Model 200{mu}m flux for an interstellar density of 0 H atom/cm^3 Jy S200,0,P Model 200{mu}m flux for ID=0 H atom/cm^3, measured within a beam of 90 arcsec Jy S200,1,T Model 200{mu}m flux for an interstellar density of 1 H atom/cm^3 Jy S200,1,P Model 200{mu}m flux for ID=1 H atom/cm^3, measured within a beam of 90 arcsec Jy S200,10,T Model 200{mu}m flux for an interstellar density of 10 H atom/cm^3 Jy S200,10,P Model 200{mu}m flux for ID=10 H atom/cm^3, measured within a beam of 90 arcsec Jy Comparison of 400, 800, 1100 and 1300 micron observed fluxes and model predictions Model Grain model 1: Jones and Merrill (1976); 2: table8 --- Name Star name --- Phase Phase of the variable star --- l_S400 Limit flag on S400 --- S400 Flux at 400{mu}m, measured through a beam of 37 arcsec Jy S400,0,T Model 400{mu}m flux for an interstellar density of 0 H atom/cm^3 Jy S400,0,P Model 400{mu}m flux for an ID=0 H atom/cm^3, measured within a beam of 37 arcsec Jy S400,1,T Model 400{mu}m flux for an interstellar density of 1 H atom/cm^3 Jy S400,1,P Model 400{mu}m flux for an ID=1 H atom/cm^3, measured within a beam of 37 arcsec Jy S400,10,T Model 400{mu}m flux for an interstellar density of 10 H atom/cm^3 Jy S400,10,P Model 400{mu}m flux for an ID=10 H atom/cm^3, measured within a beam of 37 arcsec Jy S800 Flux at 800{mu}m, measured through a beam of 16 arcsec Jy S800,0,T Model 800{mu}m flux for an interstellar density of 0 H atom/cm^3 Jy S800,0,P Model 800{mu}m flux for an ID=0 H atom/cm^3, measured within a beam of 16 arcsec Jy S800,1,T Model 800{mu}m flux for an interstellar density of 1 H atom/cm^3 Jy S800,1,P Model 800{mu}m flux for an ID=1 H atom/cm^3, measured within a beam of 16 arcsec Jy S800,10,T Model 800{mu}m flux for an interstellar density of 10 H atom/cm^3 Jy S800,10,P Model 800{mu}m flux for an ID=10 H atom/cm^3, measured within a beam of 16 arcsec Jy S1.1 Flux at 1.1mm, measured through a beam of 19 arcsec Jy S1.1,0,T Model 1.1mm flux for an interstellar density of 0 H atom/cm^3 Jy S1.1,0,P Model 1.1mm flux for an ID=0 H atom/cm^3, measured within a beam of 19 arcsec Jy S1.1,1,T Model 1.1mm flux for an interstellar density of 1 H atom/cm^3 Jy S1.1,1,P Model 1.1mm flux for an ID=1 H atom/cm^3, measured within a beam of 19 arcsec Jy S1.1,10,T Model 1.1mm flux for an interstellar density of 10 H atom/cm^3 Jy S1.1,10,P Model 1.1mm flux for an ID=10 H atom/cm^3, measured within a beam of 19 arcsec Jy S1.3 Flux at 1.3mm, measured through a beam of phi (11" or 24", see n_S1300) Jy n_S1.3 Note on S1300. 1: phi = 24"; 2: phi = 11" --- S1.3,0,T Model 1.3mm flux for an interstellar density of 0 H atom/cm^3 Jy S1.3,0,P2 Model 1.3mm flux for an ID=0 H atom/cm^3, measured within a beam of 24 arcsec Jy S1.3,0,P1 Model 1.3mm flux for an ID=0 H atom/cm^3, measured within a beam of 11 arcsec Jy S1.3,1,T Model 1.3mm flux for an interstellar density of 1 H atom/cm^3 Jy S1.3,1,P2 Model 1.3mm flux for an ID=1 H atom/cm^3, measured within a beam of 24 arcsec Jy S1.3,1,P1 Model 1.3mm flux for an ID=1 H atom/cm^3, measured within a beam of 11 arcsec Jy S1.3,10,T Model 1.3mm flux for an interstellar density of 10 H atom/cm^3 Jy S1.3,10,P2 Model 1.3mm flux for an ID=10 H atom/cm^3, measured within a beam of 24 arcsec Jy S1.3,10,P1 Model 1.3mm flux for an ID=10 H atom/cm^3, measured within a beam of 11 arcsec Jy Optical parameters of "dirty silicate" grains adapted from Jones & Merrill (1976ApJ...209..509J) lambda Wavelength um Qabs Absorption efficiency factor --- Qsca Scattering efficiency factor --- g Asymmetry parameter --- table1.tex LaTeX version of table1 table2a.tex LaTeX version of table2a table2b.tex LaTeX version of table2b table3.tex LaTeX version of table3 table6.tex LaTeX version of table6 table7.tex LaTeX version of table7 table8.tex LaTeX version of table8 Patricia Bauer CDS 1996 Apr 24 Thibaut Le Bertre, <LEBERTRE@mesioa.obspm.fr> J_A+A_314_896.xml Two dwarf galaxies in Orion with low radial velocities. J/A+A/315/348 J/A+A/315/348 BVI photometry of two Orion galaxies Two dwarf galaxies in Orion with low radial velocities. I Karachentsev I Musella Astron. Astrophys. 315 348 1996 1996A&A...315..348K Galaxies, photometry galaxies: distances and redshifts galaxies: individual (A0554+0728, ORION 0542+0502) galaxies: irregular Two relatively faint (B=15.7 and B=18.4mag, respectively), low velocity (+276 and +322km/s) galaxies were imaged with a CCD in the B, V, I bands. By means of the brightest stars we estimated their distances to be 6.4 and 5.5(+/-2)Mpc, assuming a galactic extinction of 2.7 and 2.9mag, respectively. We note that these isolated irregular dwarfs are located to a high Supergalactic latitude, -63deg, and their low radial velocities may be the result of a retarded expansion along the polar axis of the Local cloud of galaxies.
ORION galaxy Anon 0542+0502 05 45 02 +05 03 41 Anon 0554+0728 Anon 0554+07 05 57 33 +07 29 00
BVI photometry of resolved stars in the field of the ORION galaxy BVI photometry of resolved stars in the field of the A0554 galaxy Seq Star running number number=1 In tablea1: Star 75=B1, 45=B2, 114=B3, 108=B4, 15=B5. Magnitude of the star 98 is affected by bad pixels and the objects 65, 73, and 107 look like compact HII regions In tablea2: Star 28=B1, 39=B2, 47=B3, 34=B4. --- Xpos Position on V CCD frame as given by ALLSTAR arcsec Ypos Position on V CCD frame as given by ALLSTAR arcsec Bmag Calibrated B magnitude mag Vmag Calibrated V magnitude mag Imag Calibrated I magnitude mag tableph.tex LaTeX version of the tables Patricia Bauer CDS 1996 May 23 Ilaria Musella <ilaria@oacosf.na.astro.it> J_A+A_315_348.xml Binarity among B-stars in NGC 6231 J/A+A/315/384 J/A+A/315/384 Binarity among B-stars in NGC 6231 Binarity among B-stars in NGC 6231 D Raboud Astron. Astrophys. 315 384 1996 1996A&A...315..384R Binaries, spectroscopic Radial velocities binaries: general binaries: spectroscopic open clusters and associations: individual (NGC 6231) techniques: radial velocities We have measured radial velocities for 53 B-type stars, between B1 and B9, in the young open cluster NGC 6231 through a cross-correlation technique with synthetic spectra. Two measurements for 36 stars of the sample were obtained with a time separation of about two years. We derived a minimum binary fraction of 52% in the considered population. The velocity determination precisions were simulated and we analysed their dependence upon the S/N ratios of the spectra and upon the stellar rotational velocities. We discuss the selection of the templates for the correlation.
Results for all programme stars Number Star number from Seggewiss (1968VeBon..79....1S) --- Vmag V magnitude mag [B-V] Color index mag Teff Effective temperature calculated number=1 See Sect. 3.2.1 of the paper. K n_Teff Remark on Teff determination number=2 The question mark in brackets indicates that the determination is possibly outside the validity range of the Q parameter (see Sect. 3.2.1). --- Vsini Rough determination of Vsini number=3 See Sect. 3.2.2. km/s r_Teff Source of the photometry and Teff number=4 GE is for the Geneva photometry, pe for UBV photoelectric and pg for UBV photographic photometry. The digits have the following significations: 1 = Teff from Spectral Type estimated from equivalent widths (Didelon 1982A&AS...50..199D) 2 = V and [B-V] from Garrison & Schild (1979AJ.....84.1020G), Teff from Van Genderen et al. (1984A&AS...58..537V) 3 = Seggewiss (1968VeBon..79....1S) 4 = V and [B-V] from Seggewiss (1968VeBon..79....1S), Teff calculated from uvby photometry (Shobbrook 1983MNRAS.205.1229S) 5 = Garrison & Schild (1979AJ.....84.1020G) 6 = V and [B-V] from Garrison & Schild (1979AJ.....84.1020G), Teff calculated from uvby photometry (Shobbrook 1983MNRAS.205.1229S) 7 = V and [B-V] from Geneva photometry, Teff from Spectral Type (Kilian et al. 1994A&A...284..437K) and Vsini from Kilian et al. (1994A&A...284..437K) 8 = V and [B-V] from Garrison & Schild (1979AJ.....84.1020G), Teff from Spectral Type (Garrison & Schild 1979AJ.....84.1020G) 9 = Heske & Wendker (1984A&AS...57..205H) --- JD Julian Date of the observation --- RV Radial velocities km/s n_RV SBII characteristic of the star number=5 See Sect. 6.1.4. --- e_RV Radial velocity uncertainties number=6 Radial velocity uncertainties, obtained from the simulations described in Sect. 4, using a fixed B1 synthetic spectrum for all cases, and adapted in order to reproduce exactly the conditions of the radial velocity determinations for the two runs (i.e. without the region between 430 nm and 440 nm, see Sect. 3.3). km/s RVdiff1 Radial velocity differences number=7 Differences between radial velocities of column RV. km/s RVdiff2 Radial velocity differences number=7 Differences between radial velocities of column RV. km/s RVdiff3 Radial velocity differences number=8 Differential radial velocities obtained without any template (see text). km/s RVdiff4 Radial velocity differences number=8 Differential radial velocities obtained without any template (see text). km/s Raboud University of Lausanne Patricia Bauer CDS 1996 May 14 Didier Raboud <Didier.Raboud@obs.unige.ch> J_A+A_315_384.xml CCD photometry of the Tucana dwarf galaxy J/A+A/315/40 J/A+A/315/40 Photometry of the Tuc dwarf galaxy CCD photometry of the Tucana dwarf galaxy I Saviane E V Held G Piotto Astron. Astrophys. 315 40 1996 1996A&A...315...40S Galaxies, photometry Photometry, CCD galaxies: fundamental parameters galaxies: individual (Tucana) galaxies: stellar content galaxies: structure Local Group We present V and I CCD photometry for ~360 stars in the recently discovered dwarf galaxy Tucana. The large field investigated and the accurate photometric calibration make our data complementary to the deeper HST photometry. From the I magnitude of the tip of the red giant branch we estimate a distance modulus (m-M)_0_=24.69+/-0.16, corresponding to 870+/-60Kpc, confirming that Tucana is an isolated dwarf spheroidal located almost at the border of the Local Group. From the color of the red giant branch tip and by direct comparison with the giant branches of galactic globular clusters we estimate a metallicity [Fe/H]=-1.8+/-0.2, with no clear indication for a metallicity spread. The color-magnitude diagram indicates that Tucana has had a single star formation burst at the epoch of the Galactic globular cluster star formation. There is no evidence for an intermediate or young stellar population. We derive the V luminosity profile, the surface density profile of resolved stars, and the structural parameters of Tucana, from which we confirm that Tucana participates to the general metallicity-surface brightness-absolute magnitude relations defined by the Galaxy and M31 dwarf spheroidal and dwarf elliptical companions.
Coordinates and photometry of the stars No Number of star --- Xpos X-coordinate of star pix Ypos Y-coordinate of star pix Imag Landolt I magnitude mag (V-I) Landolt (V-I) color mag Patricia Bauer CDS 1996 Apr 15 I. Saviane, <saviane@astrpd.pd.astro.it> J_A+A_315_40.xml The chemical compositions of three main-sequence B-type stars in the Large Magellanic Cloud J/A+A/315/95 J/A+A/315/95 Chemical compositions of 3 LMC B stars. The chemical compositions of three main-sequence B-type stars in the Large Magellanic Cloud W R J Rolleston P J F Brown P L Dufton I D Howarth Astron. Astrophys. 315 95 1996 1996A&A...315...95R Abundances Stars, pre-main sequence galaxies: abundances Magellanic Clouds stars: abundances stars: individual (LH 104-24, PS 34-16, PS 34-144) High-resolution observations of three B-type main-sequence stars in the Large Magellanic Cloud (LMC) have been obtained with the UCL echelle spectrograph on the 3.9-m Anglo-Australian Telescope. These spectra and IUE low-resolution spectroscopic data have been analysed using LTE model-atmosphere techniques, to derive stellar atmospheric parameters and chemical compositions. As these stars lie on the hydrogen burning main-sequence, their surface abundances should reflect those of the present-day interstellar medium. From a differential analysis of LH 104-24 and PS 34-16 performed relative to the Galactic B-type stars {tau} Sco and {gamma} Peg, we conclude that there exists a general heavy-element underabundance of ~0.3dex within the LMC, but there is some evidence to suggest that these stars possess different oxygen and silicon abundances. The third star, PS 34-144, exhibits chemical anomalies, with a helium underabundance of 0.5dex and a mean metal deficiency of approximately 0.8dex. We classify this object as a Helium-weak star that is a member of the LMC. However, as additional processes such as diffusion may have occurred in its atmosphere, we do not believe that element abundances derived for PS 34-144 to be representative of the progenitor interstellar material.
LMC 05 23.6 -69 45 LH 104 (LMC) (Stellar association) 05 40.1 -69 25 PS 34-16 (LMC) 05 04.6 -66 25 PS 34-144 (LMC) 05 17.1 -66 02 Gamma Peg 00 13.2 +15 11 Tau Sco 16 35.9 -28 13
Chemical composition Line Rest wavelength of absorption feature 0.1nm Species Species --- l_PS34-16 Limit flag on PS34-16 --- PS34-16 Equivalent widths for PS 34-16 0.1pm q_PS34-16 Quality flag on PS34-16 number=1 A measure of the reliability of each measurement has been estimated with: a: having a typical accuracy of 10%; b: typical accuracy of 20% and c: accuracy probably worse than 20%. A superscript P denotes that the equivalent-width estimates of Peters (1976ApJS...30..551P) have been adopted. --- l_PS34-144 Limit flag on PS34-144 --- PS34-144 Equivalent widths for PS 34-144 0.1pm q_PS34-144 Quality flag on PS34-144 number=1 A measure of the reliability of each measurement has been estimated with: a: having a typical accuracy of 10%; b: typical accuracy of 20% and c: accuracy probably worse than 20%. A superscript P denotes that the equivalent-width estimates of Peters (1976ApJS...30..551P) have been adopted. --- l_LH104-24 Limit flag on LH104-24 --- LH104-24 Equivalent widths for LH 104-24 0.1pm q_LH104-24 Quality flag on LH104-24 number=1 A measure of the reliability of each measurement has been estimated with: a: having a typical accuracy of 10%; b: typical accuracy of 20% and c: accuracy probably worse than 20%. A superscript P denotes that the equivalent-width estimates of Peters (1976ApJS...30..551P) have been adopted. --- GamPeg Equivalent widths for gamma Peg 0.1pm q_GamPeg Quality flag on GamPeg number=1 A measure of the reliability of each measurement has been estimated with: a: having a typical accuracy of 10%; b: typical accuracy of 20% and c: accuracy probably worse than 20%. A superscript P denotes that the equivalent-width estimates of Peters (1976ApJS...30..551P) have been adopted. --- TauSco Equivalent widths for tau Sco 0.1pm q_TauSco Quality flag on TauSco number=1 A measure of the reliability of each measurement has been estimated with: a: having a typical accuracy of 10%; b: typical accuracy of 20% and c: accuracy probably worse than 20%. A superscript P denotes that the equivalent-width estimates of Peters (1976ApJS...30..551P) have been adopted. --- Patricia Bauer CDS 1996 May 03 Robert Rolleston <R.Rolleston@Queens-Belfast.AC.UK> J_A+A_315_95.xml The embedded stellar population in northern NGC 6334 J/A+A/316/102 J/A+A/316/102 JHK Photometry in NGC 6334 The embedded stellar population in northern NGC 6334 M Tapia P Persi M Roth Astron. Astrophys. 316 102 1996 1996A&A...316..102T Photometry, infrared infrared: stars ISM: individual (NGC 6334) stars: formation JHK imaging photometry is reported of an area of approximately 2'x3' centred on the far infrared source NGC 6334 I with limiting magnitudes J=18.3, H=17.8 and K=16.2. More than 224 sources were detected in K-band, increasing by a factor of more than seven the number of objects found in previous near-IR surveys. Most of the sources are located in an area of about 3500 square arcsec centered around the massive young stellar object Irs1, which ionizes the compact HII region NGC 6334 F. The location of these sources and the analysis of the colour-colour and colour-magnitude diagrams suggest the presence of an embedded and young stellar cluster of size ~70" (0.6pc), and stellar density of about 1200pc^-3^. The star formation efficiency is estimated to be SFE=~0.25. Only a few of the most luminous stars of the cluster were found to show large near-IR excesses but this may be due to the non-detection, at the shortest wavelength, of the majority of the highly reddened cluster members. The extinction of the region is very variable with a maximum of A_V_>70 in Irs2 while the average is <A_V_>=~40. Very close to the position of an H_2_O maser associated with NGC 6334 I(N), a contracting core at an earlier evolutionary stage, we found six very red sources, one of which is a small and diffuse nebula seen only at 2.2{mu}m. Finally, the older and developed HII region NGC 6334 E was found to be probably ionized by a small cluster of at least 12 B0-B0.5 ZAMS stars. For a description of the JHK photometric system, see e.g. <GCPD/09>
Coordinates and photometry of sources No Identification number --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right Ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec l_Jmag Limit flag on J magnitude --- Jmag J magnitude mag l_Hmag Limit flag on H magnitude --- Hmag H magnitude mag Kmag K magnitude mag Notes See note number=1 (1) Outside J and H images. (2) Irs3. (3) Near-IR excess. (St) Straw et al. (1989ApJS...69...99S) (4) Irs1. Phot. of components, in Paper I (Persi et al., 1996A&A...307..591P) (St) Straw et al. (1989ApJS...69...99S) (*) Probable exciting star of HII region E. (Neb.) Nebular object (H2 Knot) Molecular hydrogen emission knot --- Patricia Bauer CDS 1996 Apr 15 Mauricio Tapia <mt@bufadora.astrosen.unam.mx> J_A+A_316_102.xml Optically identified QSO absorption systems and galaxy evolution J/A+A/316/123 J/A+A/316/123 QSO absorber and galaxy evolution Optically identified QSO absorption systems and galaxy evolution U Lindner U Fritze-von Alvensleben K J Fricke Astron. Astrophys. 316 123 1996 1996A&A...316..123L QSOs cosmology: observations galaxies: evolution quasars: absorption lines In this appendix we briefly comment on each paper from which we have compiled data on optically identified QSO absorption systems (cf. Section 3 of the paper published in the Main Journal).
appen.tex TeX version of appendix fig1.ps R and r apparent magnitude vs z fig2.ps R apparent magnitude vs z fig3.ps g apparent magnitude vs z fig4.ps R apparent magnitude vs z (Different H and omega) Patricia Bauer CDS 1996 Jun 10 J_A+A_316_123.xml Catalogue and luminosity function of white dwarfs detected in the ROSAT All-Sky Survey J/A+A/316/147 J/A+A/316/147 Catalogue of ROSAT White Dwarfs Catalogue and luminosity function of white dwarfs detected in the ROSAT All-Sky Survey T A Fleming S L Snowden E Pfeffermann U G Briel J Greiner Astron. Astrophys. 316 147 1996 1996A&A...316..147F IX/10 : ROSAT All-Sky Bright Source Catalogue III/129 : Catalogue of Spectroscopically Identified White Dwarfs Stars, white dwarf X-ray sources stars: statistics surveys white dwarfs X-rays: stars Table1 lists all white dwarf stars, both previously-catalogued and newly discovered, which have been detected in the ROSAT All-Sky Survey. The positions and count rates of the X-ray sources associated with each star are given, as well as spectral types and other star names for those stars which have been previously catalogued. Table2 lists distances estimated via Balmer line profile fitting, corrected (for IS absorption) X-ray luminosities, and each star's contribution to the X-ray luminosity function for all DA white dwarfs which were detected in the ROSAT All-Sky Survey.
ROSAT
All white dwarfs detected in the ROSAT PSPC Survey RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec n_Rate Note on count rate number=1 + indicates detection also made in hard band; should be treated as upper limit --- Rate PSPC count rate in the 0.1-0.28 keV band ct/s e_Rate 1-sigma error in count rate ct/s WFCflag Was source detected in EUV by ROSAT WFC? --- Name Star name --- WD Villanova catalogue designation <III/129> --- Type White dwarf spectral type --- Ref References number=2 (1) Barstow M.A. et al. (1993MNRAS.264...16B) (2) Fleming T.A. et al. (1993ApJ...416L..79F) (3) Barstow M.A. et al. (1994MNRAS.270..499B) (4) Hoare M.G. et al. (1995MNRAS.273..812H) (5) Barstow M.A. et al. (1992MNRAS.255..369B) (6) Barstow M.A. et al. (1993MNRAS.260..631B) (7) Hodgkin S.T. et al. (1993MNRAS.263..229H) (8) Barstow M.A. et al. (1995MNRAS.273..711B) (9) Tweedy R.W. et al. (1993AJ....105.1938T) (10) Fleming T.A. et al. (1991A&A...246L..47F) (11) Barstow M.A. et al. (1994MNRAS.271..175B) (12) Motch C. et al. (1993A&A...268..561M) (13) Genova R. et al. (1995AJ....110..788G) (14) Sion E.M. et al. (1995PASP..107..232S) (15) Kahabka P. et al. (1994A&A...288..538K) (16) Cowley A.P. et al. (1995PASP..107..927C) --- Adopted distances, X-ray luminosities, and contributions to the luminosity function for the ROSAT DA stars Name Star name or RASS designation --- n_Name Note on RX J2034.9-2734 number=1 For RX J2034.9-2734, neither photometry nor good spectrum available --- n_Dist An '*' indicates distance estimated assuming M_V_ = 9.63 --- Dist Distance estimated to each star pc Lx' Corrected X-ray luminosity (0.1-0.28 keV) 10-7W 1/Va' Each star's contribution to the LF and local space density pc-3 table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 Thomas A. Fleming Steward Obs. Patricia Bauer CDS 1996 Jul 23 Thomas A. Fleming <taf@as.arizona.edu> J_A+A_316_147.xml ROSAT PSPC survey of M 31 J/A+A/317/328 J/A+A/317/328 ROSAT PSPC survey of M 31 ROSAT PSPC survey of M 31 R Supper G Hasinger W Pietsch J Truemper A Jain E A Magnier W H G Lewin J Van Paradijs Astron. Astrophys. 317 328 1997 1997A&A...317..328S Infrared sources X-ray sources galaxies: fundamental parameters galaxies: individual (M 31) galaxies: luminosity function, mass function galaxies: spiral X-rays: general This paper reports on results of the analysis of the first M 31 survey with the ROSAT PSPC performed in July 1991. Within the =~ 6.3deg^2^ field of view we detected 396 individual X-ray sources with (0.1keV-2.4keV) fluxes ranging from =~ 5x10^-15^erg/cm^2^/s^ to =~ 4x10^-12^erg/cm^2^/s. Of these 396 sources, 43 have be en tentatively identified with foreground stars, 29 with globular clusters, 17 with supernova remnants, 3 with other galaxies (including M 32), and 3 with radio sources. A detailed analysis of the integral flux distribution of the sources shows that approximately one fifth are likely to be background objects. By comparison with the results of the Einstein M 31 survey, we find 327 newly detected sources, 15 moderately variable sources, 3 bright and 6 faint possible transient sources. For those sources in M 31, the observed luminosities range from =~ 3x10^35^erg/s to =~ 2x10^38^erg/s (at 690kpc). The total (0.1keV-2.4keV) luminosity of M 31 is (2.9+/-0.3)x10^39^erg/s, roughly one third of which is from the bulge and two thirds of which are from the disk. The luminosity of a diffuse component within the bulge region is estimated to be less than 3.2x10^38^erg/s. An explanation in terms of hot gaseous emission leads to a maximum total gas mass of 1.7x10^6^M_{sun}_. We find that the integral luminosity distribution of sources associated with globular clusters is similar to that of the Milky Way. Finally, the results of spectral fits to 56 of the brightest sources are discussed; we classify 15 objects as "supersoft sources" according to their spectral characteristics.
ROSAT
List of all 396 ROSAT sources found in M31 n_ROSAT Note on ROSAT source number number=1 a: Galactic foreground star b: Background galaxy c: Radio source d: Globular cluster e: SNR *: bulge source +: Sources with uncertain count rate --- ROSAT ROSAT source number --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec e_DEs 1 sigma position error arcsec Cl Source classification number=2 The X-ray sources are classified due to the quality of their detection, which has an influence on the determined properties: 1 = best, 2 = medium, 3 = moderate. --- MaxL Maximum likehood --- Band Energy band with highest detection number=3 The ROSAT energy bands are coded within this paper as: B = Broad = 0.1-2.4 keV S = Soft = 0.1-0.4 keV H1 = Hard1 = 0.5-0.9 keV H2 = Hard2 = 0.9-2.0 keV H = Hard = 0.5-2.0 keV (= H1 + H2). --- l_rateB Limit flag on rate B number=4 For sources not detected in a considered energy band 1{sigma} upper limits have been calculated indicated by a `<`-symbol in front of the upper limit value. --- rateB Count rate in the B-band ct/ks e_rateB rms uncertainty on rateB number=5 The listed count rate errors are only statistical. The systematic errors are expected to be less than ~15%. A conversion of count rates into fluxes depends on the assumed spectral shape. For M31-sources a power law with {Gamma}=-2.0 and N_H_=9x10^20^cm^-2^ may be used, leading to the conversion factor 1cts/ks=3.12x10^-14^erg/cm^2^/s in the 0.1-2.4keV band (B-band). For foreground stars the application of this conversion factor leads to an over-estimate of the fluxes. ct/ks l_rateS Limit flag on rate S number=4 For sources not detected in a considered energy band 1{sigma} upper limits have been calculated indicated by a `<`-symbol in front of the upper limit value. --- rateS Count rate in the S-band ct/ks e_rateS rms uncertainty on rateS number=5 The listed count rate errors are only statistical. The systematic errors are expected to be less than ~15%. A conversion of count rates into fluxes depends on the assumed spectral shape. For M31-sources a power law with {Gamma}=-2.0 and N_H_=9x10^20^cm^-2^ may be used, leading to the conversion factor 1cts/ks=3.12x10^-14^erg/cm^2^/s in the 0.1-2.4keV band (B-band). For foreground stars the application of this conversion factor leads to an over-estimate of the fluxes. ct/ks l_rateH Limit flag on rate H number=4 For sources not detected in a considered energy band 1{sigma} upper limits have been calculated indicated by a `<`-symbol in front of the upper limit value. --- rateH Count rate in the H-band ct/ks e_rateH rms uncertainty on rateH number=5 The listed count rate errors are only statistical. The systematic errors are expected to be less than ~15%. A conversion of count rates into fluxes depends on the assumed spectral shape. For M31-sources a power law with {Gamma}=-2.0 and N_H_=9x10^20^cm^-2^ may be used, leading to the conversion factor 1cts/ks=3.12x10^-14^erg/cm^2^/s in the 0.1-2.4keV band (B-band). For foreground stars the application of this conversion factor leads to an over-estimate of the fluxes. ct/ks l_rateH1 Limit flag on rate H1 number=4 For sources not detected in a considered energy band 1{sigma} upper limits have been calculated indicated by a `<`-symbol in front of the upper limit value. --- rateH1 Count rate in the H1-band ct/ks e_rateH1 rms uncertainty on rateH1 number=5 The listed count rate errors are only statistical. The systematic errors are expected to be less than ~15%. A conversion of count rates into fluxes depends on the assumed spectral shape. For M31-sources a power law with {Gamma}=-2.0 and N_H_=9x10^20^cm^-2^ may be used, leading to the conversion factor 1cts/ks=3.12x10^-14^erg/cm^2^/s in the 0.1-2.4keV band (B-band). For foreground stars the application of this conversion factor leads to an over-estimate of the fluxes. ct/ks l_rateH2 Limit flag on rate H2 number=4 For sources not detected in a considered energy band 1{sigma} upper limits have been calculated indicated by a `<`-symbol in front of the upper limit value. --- rateH2 Count rate in the H2-band ct/ks e_rateH2 rms uncertainty on rateH2 number=5 The listed count rate errors are only statistical. The systematic errors are expected to be less than ~15%. A conversion of count rates into fluxes depends on the assumed spectral shape. For M31-sources a power law with {Gamma}=-2.0 and N_H_=9x10^20^cm^-2^ may be used, leading to the conversion factor 1cts/ks=3.12x10^-14^erg/cm^2^/s in the 0.1-2.4keV band (B-band). For foreground stars the application of this conversion factor leads to an over-estimate of the fluxes. ct/ks Correlation with the Einstein source catalog n_ROSAT Note on ROSAT source number number=1 ROSAT source numbers marked with a star are bulge sources for which the fluxes and variabilities could be overestimated. --- ROSAT ROSAT source number --- FR Source flux measured by ROSAT number=2 Source flux obtained by applying the spectral model of TF (thermal bremsstrahlung with kT=5keV and N_H_=7x10^20^cm^-2^) in the 0.2-4.0keV energy band. 0.1fW/m2 e_FR rms uncertainty on FR 0.1fW/m2 Einst. Einstein source number --- FE Source flux measured by Einstein number=2 Source flux obtained by applying the spectral model of TF (thermal bremsstrahlung with kT=5keV and N_H_=7x10^20^cm^-2^) in the 0.2-4.0keV energy band. 0.1fW/m2 e_FE rms uncertainty on FE 0.1fW/m2 Dist Distance between sources arcsec Dists Distance between sources in sigma number=3 Expressed in sigma of their combined 1 sigma position error. --- FR/FE ROSAT-Eintein source flux ratio --- e_FR/FE rms uncertainty on FR/FE number=4 Gaussian error propagation used. --- Correlations with different data bases ROSAT ROSAT source number --- DataBase Data base with correlations number=1 For a detailed description of the used data bases see printed paper. Here a short listing: BA87, BA93 = Globular cluster lists of Battistini et al. (1987A&AS...67..447B) Battistini et al. (1993A&A...272...77B) BW93 = SNR-list of Braun & Walterbos (1993A&AS...98..327B) DO80 = SNR-list of d'Odorico et al. (1980A&AS...40...67D) MA92 = Foreground star catalogs by Magnier et al. (1992A&AS...96..379M) Haiman et al. (1994A&A...286..725H) MA94b = SNR-list of Magnier et al., 1994, A&AS, submitted NED = NASA Extragalactic Database (Version 30.Dec.1992) SIMBAD = SIMBAD catalog (Centre de Donnees astronomiques de Strasbourg, Version Dec.1989) --- Dist1 Distance between sources in arcsec arcsec Dist2 Distance between sources in arcsec number=2 When more than one data base are listed in Data_Base arcsec Dist3 Distance between sources in arcsec number=2 When more than one data base are listed in Data_Base arcsec Dist1s Distance 1 between sources in sigma number=3 Expressed in sigma of their combined 1 sigma position error. --- Dist2s Distance 2 between sources in sigma number=3 Expressed in sigma of their combined 1 sigma position error. --- Dist3s Distance 3 between sources in sigma number=3 Expressed in sigma of their combined 1 sigma position error. --- Id Identification --- Type Type (star, galaxy, SNR, cluster) --- Spectral fit parameters of 56 bright X-ray sources n_ROSAT Note on ROSAT source number number=1 a: Galactic foreground star b: Background galaxy d: Globular cluster e: SNR *: bulge source --- ROSAT ROSAT source number --- Circle Photon collection circle number=2 Expressed in sigma of the point spread function of the intrumentation ROSAT XRT+PSPC. --- Counts Number of photons used for the fit --- NH1 Hydrogen abs. column density for Gamma 10+20cm-2 E_NH1 Error in NH1 (upper limit) 10+20cm-2 e_NH1 Error in NH1 (lower limit) 10+20cm-2 Gamma Power law index --- E_Gamma Error in Gamma (upper limit) --- e_Gamma Error in Gamma (lower limit) --- 2_Gamma Reduced Chi2 for Gamma --- NH2 Hydrogen absolute column density for Thermal Bremsstrahlung fit 10+20cm-2 E_NH2 Error in NH2 (upper limit) 10+20cm-2 e_NH2 Error in NH2 (lower limit) 10+20cm-2 kT1 Thermal Bremsstrahlung temperature keV E_kT1 Error in kT1 (upper limit) keV e_kT1 Error in kT1 (lower limit) keV 2_kT1 Reduced Chi2 for kT1 --- Fit Spectral fit model indicator (3) B: Black body; T: Thermal plasma --- NH3 Hydrogen column density for Fit 10+20cm-2 E_NH3 Error in NH3 (upper limit) 10+20cm-2 e_NH3 Error in NH3 (lower limit) 10+20cm-2 kT2 Thermal Plasma/Blackbody temperature keV E_kT2 Error in kT2 (upper limit) keV e_kT2 Error in kT2 (lower limit) keV 2_Fit Reduced Chi2 for Fit --- *Power law fit parameters with fixed NH n_ROSAT Note on ROSAT source number number=1 d: Globular cluster e: SNR *: bulge source --- ROSAT ROSAT source number --- Gamma Power law index --- e_Gamma rms uncertainty on Gamma --- 2_Gamma Reduced Chi2 for Gamma --- tables.tex LaTeX (with supertabular) version of tables Patricia Bauer CDS 1996 Apr 22 J_A+A_317_328.xml Physical conditions in metal line systems toward Q1037-2704: Evidence for superclustering at z ~ 2. J/A+A/317/416 J/A+A/317/416 Superclustering in the field of Q1037-2704 Physical conditions in metal line systems toward Q1037-2704: Evidence for superclustering at z ~ 2. Y Lespine P Petitjean Astron. Astrophys. 317 416 1997 1997A&A...317..416L Line Profiles QSOs galaxies: formation intergalactic medium large-scale structure of universe quasars: absorption lines quasars: individual (Q1037-2704) The table gives the characteristics of the absorption lines observed in the spectrum of Q1037-2704 from 3733 A to 5050 A.
QSO 1037-2704 10 39 21.8 -27 19 15.8
Absorption lines No Numbering of the line as indicated in Fig. 1 of the paper --- Lambda Vacuum heliocentric wavelength 0.1nm u_Lambda Uncertainty flag on LambdaHelio --- Wobs Observed wavelength 0.1nm u_Wobs Uncertainty flag on Wobs --- e_Wobs 1 sigma error in the continuum number=1 sigmaWobs = {sigma} x FWHM where {sigma} is the noise rms in the adjacent continuum 0.1nm Ident Identification --- Zabs Mean redshift of the line --- nFit Number of components used to fit the line --- log(N) Logarithm of the column density cm-2 n_log(N) Note on log(N) number=2 Uncertain determination: typical error is 0.5 instead of 0.15 for other lines --- b Doppler parameter km/s u_b Uncertainty flag on b --- z Redshift of the component (upper limit) --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 Jun 18 Patrick Petitjean <ppetitje@iap.fr> J_A+A_317_416.xml Be star surveys with CCD photometry. II. NGC 1818 and its neighbouring cluster in the LMC. J/A+A/317/448 J/A+A/317/448 BVRHalpha photometry of NGC 1818 Be star surveys with CCD photometry. II. NGC 1818 and its neighbouring cluster in the LMC. E K Grebel Astron. Astrophys. 317 448 1997 1997A&A...317..448G Clusters, globular Photometry, CCD galaxies: star clusters globular clusters: individual (NGC 1818) Magellanic Clouds stars: emission-line, Be stars: fundamental parameters We present B,V,R,Halpha CCD photometry and astrometry of Be stars in NGC 1818, its small neighbouring cluster NGC 1818B, and the surrounding field down to V = 18 mag. Our Be star identifiers conform to IAU specifications. For a description of the UBVRI and Halpha systems, see e.g. <GCPD/08> and <GCPD/55>
Identifiers, photometry, astrometry of Be stars in NGC 1818 and surroundings ID Be star identifier following IAU specs. --- Rob Identifiers from Robertson (1974) --- Will Identifiers from Will et al. (1995) --- Loc Location: A = Be star in NGC 1818, B = NGC 1818B, F = field --- Dist Distance from the center of NGC 1818 arcsec Vmag V magnitude mag e_Vmag Photometric error of the V magnitude mag B-V (B-V) colour mag e_B-V Photometric error of the (B-V) colour mag R-Halpha (R-Halpha) colour mag e_R-Halpha Photometric error of the (R-Halpha) colour mag RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Patricia Bauer CDS 1996 Jun 18 E.K. Grebel <grebel@astro.uiuc.edu> J_A+A_317_448.xml IRC+10 216 revisited I: the circumstellar dust shell J/A+A/317/503 J/A+A/317/503 Photometric & visibility data of IRC +10 216 IRC+10 216 revisited I: the circumstellar dust shell M A T Groenewegen Astron. Astrophys. 317 503 1997 1997A&A...317..503G Infrared sources Stars, variable circumstellar matter infrared: stars stars: AGB and post-AGB stars: individual (IRC +10 216) stars: mass-loss A spherically symmetric dust radiative transfer code is used to model the circumstellar dust shell around IRC +10 216. Compared to numerous previous models a much larger body of observational data is used as constraints; the spectral energy distribution between 0.5 and 60000{mu}m, 2-4{mu}m and 8-23{mu}m spectra, optical, far-infrared and centimeter sizes and interferometric visibility curves between 1.6 and 11.2{mu}m are used to constrain the model. The most important result is that in order to fit the visibility curve at 2.2{mu}m and the size of the shell in the optical, scattering has to be invoked.
IRC +10216 CW Leo 09 47 57.2 +13 16 44
Summary of existing models of IRC +10 216 Ref Reference number=1 The references are: MR80 = Mitchell & Robinson (1980MNRAS.190..669M) RRH83 = Rowan-Robinson & Harris (1983MNRAS.202..797R) MR87 = Martin & Rogers (1987ApJ...322..374M) LB87 = Le Bertre (1987A&A...176..107L) LB88 = Le Bertre (1988A&A...203...85L) RK88 = Ridgway & Keady (1988ApJ...326..843R) G90 = Griffin (1990MNRAS.247..591G) O90 = Orofino et al. (1990A&A...231..105O) LML93 = Lorenz-Martins & Lefevre (1993A&A...280..567L) D94 = Danchi et al. (1994AJ....107.1469D) W94 = Winters et al. (1994A&A...288..255W) B95 = Bagnulo et al. (1995A&A...301..501B) IE96 = Ivezic & Elitzur (1996MNRAS.279.1011I) --- Teff Effective temperature or lowest value if interval of the central star K n_Teff Note on Teff number=2 A means that the parameter value was assumed - indicates an interval ? for unknown value --- Teff2 Highest effective temperature when interval --- Depth Optical depth --- Radc Inner radius or lowest value if interval of the dust shell in stellar radii --- n_Radc Note on Radc number=2 A means that the parameter value was assumed - indicates an interval ? for unknown value --- Radc2 Highest inner radius when interval --- Tc Dust temperature at the inner dust radius K n_Tc Note on Tc number=2 A means that the parameter value was assumed - indicates an interval ? for unknown value --- Grains Type of grain used --- DensLaw r power number of the density law --- n_DensLaw Note on DensLaw number=3 b: fpr r<=10R* c: Calculated from first principle e: Density distribution calculated taking a constant mass lost rate and a hydrodynamical calculation to determine the velocity law --- L/D2 Luminosity versus square distance solLum/kpc2 n_L/D2 '?' for unknown value --- Const Constraints used number=4 SED = spectral energy distribution LRS = low resolution spectrograph --- Photometric data used in the modeling Ref Reference --- Lambda Wavelength um n_Lambda '-' when interval --- Lambda2 Highest wavelength when interval um Flux Flux (see unit in X_Flux) --- e_Flux rms uncertainty on Flux --- x_Flux Units of flux and e_Flux --- Beam Beam size arcsec n_Beam for unknown value; x for box beam --- Beam2 Second value when box beam (AxB) arcsec Phase Phase number=1 The phase is calculated adopting a period of 649 days and maximum light (phase=0.0) at JD = 2447483 (Le Bertre, 1992A&AS...94..377L). --- n_Phase ? for unknown value; - when interval --- Phase2 Highest values when interval --- Rem Remarks --- Visibility data Lambda Wavelength um Ref Reference --- Phase1 Phase number=1 The phase is calculated adopting a period of 649 days and maximum light (phase = 0.0) at JD = 2447483 (Le Bertre, 1992A&AS...94..377L). --- n_Phase1 '-' when interval --- Phase1b Upper value when interval --- Phase2 Second values for the phase --- Phase3 Third values for the phase --- Rem Remarks --- appen.tex LaTeX version of Appendix tables.tex LaTeX version of the tables fig11.ps Geometry of the problem Patricia Bauer CDS 1996 Jun 07 Martin Groenewegen <groen@MPA-Garching.MPG.DE> J_A+A_317_503.xml Globular clusters 1 and 3 in the Fornax dwarf galaxy J/A+A/317/54 J/A+A/317/54 Fornax cluster 1 and 3 photometry Globular clusters 1 and 3 in the Fornax dwarf galaxy U G Jorgensen R Jimemez Astron. Astrophys. 317 54 1997 1997A&A...317...54J Clusters, globular Photometry, CCD galaxies: formation galaxies: individual (Fornax dSph, A0237-34) galaxies: star clusters stars: AGB and post-AGB stars: carbon We have performed photometric CCD observations of the giant and horizontal branches of the globular cluster1, and of the giant branch of cluster3, in the Fornax dwarf spheroidal galaxy. The observations were performed in the V and I standard broad-band filters as well as through two narrow-band filters especially designed to distinguish between carbon and M type stars. The AGB is richly populated with carbon-rich stars, and all of them are considerably below the theoretical lower luminosity limit for such stars. If the Fornax clusters are interpreted as resembling an earlier epoch of the Galactic globular clusters, the low luminosities of the carbon stars therefore point to a larger role of the low-mass stars in the chemical enrichment of our Galaxy. The giant branches of the Fornax clusters are much broader than canonical giant branches in Galactic globulars, and the AGB is more well populated. We suggest that the morphology and stellar population of the giant branches indicate that the dwarf galaxies are =~3Gyr younger than the Galactic halo, which in turn seems to be =~3Gyr younger than the Galactic globular clusters. For a description of the N2-N3 photometric system, see e.g. <GCPD/39>
Cluster 1 in Fornax 02 37.0 -34 11 Cluster 3 in Fornax 02 39.8 -34 16
Cluster 1 photometry Cluster 3 photometry ID Identification number --- Vmag V magnitude mag B-V B-V color index mag logL Reduced luminosity solLum logTeff Effective temperature K Mbol Absolute bolometric magnitude mag 81-78 Narrow band color {DELTA}m_(81-78)_=m(8120A)-m(7795A) mag N2 Number in Buonanno et al. (1985) catalogue --- Vmag2 V magnitude in Buonanno et al. (1985) mag N3 Number in Demers et al. (1990) catalogue number=1 These data are only in table1 --- Vmag3 V magnitude in Demers et al. (1990) number=1 These data are only in table1 mag tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Jun 03 Raul Jimenez <R.Jimenez@roe.ac.uk> J_A+A_317_54.xml Proper motion of the hot subdwarfs. The kinematic population membership of the SdB J/A+A/317/689 J/A+A/317/689 Hot subdwarfs proper motions Proper motion of the hot subdwarfs. The kinematic population membership of the SdB P Thejll C Flynn R Williamson R Saffer Astron. Astrophys. 317 689 1997 1997A&A...317..689T Proper motions Stars, subdwarf astrometry stars: fundamental parameters Galaxy: stellar content subdwarfs We report on first results from an ongoing program to measure and analyze proper motions for hot subdwarf and white dwarf stars, with the aim of determining to which stellar population sdB stars (in the V magnitude range 10.5 to 14.5) belong. Ours is the largest sample of hot subdwarf proper motions measured to date. Our kinematic analysis suggests that the parent population of these hydrogen-rich sdB stars is as old or older than the old disk. We measure the absolute magnitude of the sdB in the field as M_V_=4.5, providing independent confirmation of absolute V magnitude estimates for these stars from clusters and spectroscopic analyses. Provided it can be shown that the sdO stars evolve from the sdB, then the sdO absolute V magnitude distribution is about 1 magnitude brighter than for the sdB, and 1 magnitude wider.
Astrometric results for the hot subdwarfs (table4 to 9 of the paper) RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec pm1 Proper motion from the AC/CAMC system arcsec/yr e_pm1 rms uncertainty on pm1 arcsec/yr PA1 Position angle for proper motion from the AC/CAMC system (counted positive east of north) deg e_PA1 rms uncertainty on PA1 deg pm2 Proper motion from the POSS/GSC system arcsec/yr e_pm2 rms uncertainty on pm2 arcsec/yr PA2 Position angle for proper motion from the POSS/GSC system (counted positive east of north) deg e_PA2 rms uncertainty on PA2 deg Note Note --- White dwarf astrometric results from the AC/CAMC and the POSS/GSC efforts (table10 & 11 of the paper) RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec pm Proper motion arcsec/yr e_pm rms uncertainty on pm arcsec/yr PA Position angle for proper motion (counted positive east of north) deg e_PA rms uncertainty on PA deg Class WD Spectral class number=1 WD spectral class derived from positions and the WD catalog <III/129> --- Name Various names for the star taken from the McCook & Sion catalog. number=2 PG and KPD refers to stars in Green et al. (1986) and Downes (1986). --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Aug 01 Peter A. Thejll <thejll@nordita.dk> J_A+A_317_689.xml The 1978-1995 variability of the symbiotic star AG Pegasi in the ultraviolet J/A+A/317/712 J/A+A/317/712 UV fluxes and electron density of AG Peg The 1978-1995 variability of the symbiotic star AG Pegasi in the ultraviolet A Altamore A Cassatella Astron. Astrophys. 317 712 1997 1997A&A...317..712A Binaries, cataclysmic Energy distributions Spectra, ultraviolet binaries: symbiotic line: profiles novae, cataclysmic variables stars: individual (AG Peg) ultraviolet: stars In this paper we study in detail the variability of the symbiotic nova AG Peg in the IUE range during the period 1978-1995. We find that the luminosity of the hot component decreased steadily from about 1850L_{sun}_ in 1978 to 430L_{sun}_ in 1995 while its effective temperature remained nearly constant, 86500+/-1300K. At the same time, the mass loss rate decreased by a factor of 4-5 although the ejection velocity remained constant. The observed fainting of both the narrow and the broad emission lines is ascribed to the decrease of the luminosity and ionizing flux from the hot source. The narrow emission lines and the long wavelength UV continuum show periodic variations arising from a dense and asymmetric nebular region associated with the cool star. Radial velocity variations of the narrow lines indicate that this region is receding from the center of mass of the system, and support the presence of the ablation tail suggested by Penston and Allen (1985MNRAS.212..939P). No periodic flux variations are seen in the short wavelength ultraviolet continuum and in the broad emission lines, which are both formed in the fast wind from the hot component.
AG Peg 21 51 01.9 +12 37 32
FES magnitudes and UV fluxes HJD Julian date d FESmag Fine Error Sensor magnitude mag F1455 Observed flux at 1455 A number=1 Fluxes are in 10**(-13) erg/cm2/s/A. 10-15W/m2/nm F1835 Observed flux at 1835 A number=1 Fluxes are in 10**(-13) erg/cm2/s/A. 10-15W/m2/nm F2855 Observed flux at 2855 A number=1 Fluxes are in 10**(-13) erg/cm2/s/A. 10-15W/m2/nm Electron density from the [SiIII]/[CIII] ratio HJD Julian date d FSiIII Observed flux of SiIII] 1893 A line number=1 Fluxes are in 10**(-11) erg/cm2/s 10-14W/m2 FCIII Observed flux of CIII] 1909 A line (1)9 10-14W/m2 log(Ne) Decimal log of electron density cm-3 Electron density from the [N III] multiplet HJD Julian date d F1748.6 Observed flux of N III] 1748.6 A line number=1 Fluxes are in 10**(-11) erg/cm2/s 10-14W/m2 F1749.5 Observed flux of N III] 1749.5 A line number=1 Fluxes are in 10**(-11) erg/cm2/s 10-14W/m2 F1754.0 Observed flux of N III] 1754.0 A line number=1 Fluxes are in 10**(-11) erg/cm2/s 10-14W/m2 log(Ne) Decimal log of electron density cm-3 Radial velocities of the UV emission lines HJD Julian date d HRV Mean heliocentric radial velocity of the CIII] and SiIII] lines km/s e_HRV rms uncertainty on HRV1 km/s RV1 Radial velocity of the HeII 1640A emission line km/s RV2 Radial velocity of the NIV] 1487A emission line km/s HeII Zanstra temperatures Note H: High resolution data, L: Low resolution data --- HJD Julian date d F1640 Flux of the HeII 1640A line number=1 Fluxes are in 10**(-11) erg/cm2/s 10-14W/m2 F1335 Flux of the continuum around 1335A number=2 Fluxes are in 10**(-11) erg/cm2/s/A 10-13W/m2/nm F1640/F1335 Ratio of F1640 to F1335 --- T Zanstra temperature K table2.tex TeX version of table2 table3a.tex TeX version of table3a table3b.tex TeX version of table3b table4.tex TeX version of table4 table5.tex TeX version of table5 Patricia Bauer CDS 1996 Nov 06 Angelo Cassatella <CASSATELLA@amaldi.fis.uniroma3.it> J_A+A_317_712.xml Determination of Miras temperatures from TiO and VO bands. Estimates of distances. J/A+A/317/761 J/A+A/317/761 Miras temperatures, distances & magnitudes Determination of Miras temperatures from TiO and VO bands. Estimates of distances. R Alvarez M -O Mennessier Astron. Astrophys. 317 761 1997 1997A&A...317..761A Models, atmosphere Stars, variable stars: AGB and post-AGB stars: atmospheres stars: distances stars: fundamental parameters Effective temperatures are determined for a sample of 165 oxygen-rich Miras using indices related to molecular band strength of titanium oxide and vanadium oxide. Using a theoretical evolutionary track on AGB, absolute bolometric magnitudes are computed. Apparent bolometric magnitudes are determined from narrow-band photometry observations. They are used to calibrate distances.
Fundamental parameters GCVS Name --- P Period d Group Group --- T Temperature K e_T Uncertainty on temperature K Amp Amplitude of temperature variation K Mbol Absolute bolometric magnitudes mag mbol Apparent bolometric magnitudes mag Dist Distance pc Type Mira type, see Note number=1 the type is defined as: H: Miras classified as halo stars by Luri et al. (1996A&AS..117..405L) SP: Short-period Miras not belonging to the sample of Luri et al. MS: MS-Miras --- Alvarez GRAAL Patricia Bauer CDS 1996 Jun 10 R. Alvarez <alvarez@graal.univ-montp2.fr> J_A+A_317_761.xml The ROSAT Galactic Plane Survey: analysis of a low latitude sample area in Cygnus. J/A+A/318/111 J/A+A/318/111 ROSAT Galactic Plane Survey The ROSAT Galactic Plane Survey: analysis of a low latitude sample area in Cygnus. C Motch P Guillout F Haberl M W Pakull W Pietsch K Reinsch Astron. Astrophys. 318 111 1997 1997A&A...318..111M IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) J/A+AS/122/201 : ROSAT Galactic Plane Survey observations (Motch+ 1997) X-ray sources stars: activity stars: neutron stars: statistics X-rays: general X-rays: stars We present the analysis of the point source content of a low galactic latitude region selected from the ROSAT all-sky survey. The test field is centered at l=90, b=0 and has an area of 64.5deg^2^. A total of 128 soft X-ray sources are detected above a maximum likelihood of 8. Catalogue searches and optical follow-up observations show that in this direction of the galactic plane, 85% of the sources brighter than 0.03PSPC are identified with active coronae. F-K type stars represent 67% (+/-13%) of the stellar identifications and M type stars account for 19% (+/-6%). A small but significant number of X-ray sources are associated with A type stars on the basis of positional coincidence. These results together with those of similar optical campaigns demonstrate that the soft X-ray population of the Milky Way is largely dominated by active stars. We show that the density and distribution in flux and spectral type of the active coronae detected in X-rays are consistent with the picture drawn from current stellar population models and age dependent X-ray luminosity functions. The modelling of this population suggests that most of the stars detected by ROSAT in this direction are younger than 1Gyr. This opens the possibility to extract in a novel way large samples of young stars from the ROSAT all-sky survey. The small number of unidentified sources at low X-ray flux put rather strong constraints on the hypothetical X-ray emission from old neutron stars accreting from the interstellar medium. Our observations clearly rule out models which assume no dynamical heating for this population and a total number of N_ns_=10^9^ neutron stars in the Galaxy. If accretion on polar caps is the dominant mode then our upper limit may imply N_ns_=~10^8^. Among the non coronal identifications are three white dwarfs, a Seyfert 1 active nucleus, two early type stars and one cataclysmic variable. We also report the discovery of a Me+WD close binary system with P_orb_=~12 .
ROSAT
Optical identifications for sources with ML>=8 Optical identifications for sources with 7>=ML>=8 Source Source index --- ROSAT ROSAT name --- Class Class of the proposed optical counterpart number=1 AC: active corona AGN: active galactic nucleus CV: cataclysmic variable OB: OB star WD: White dwarf ??: Unknown --- u_Class ? for the more uncertain cases number=2 Proposed counterparts having a probability of identification in the range 95% - 98%, These more uncertain cases are marked by a '?' in the u_IdOpt column and in the u_Class column --- SpType Spectral type --- IdOpt Optical identification number=2 Proposed counterparts having a probability of identification in the range 95% - 98%, These more uncertain cases are marked by a '?' in the u_IdOpt column and in the u_Class column --- u_IdOpt ? for the more uncertain cases number=2 Proposed counterparts having a probability of identification in the range 95% - 98%, These more uncertain cases are marked by a '?' in the u_IdOpt column and in the u_Class column --- Count Count rate ct/s e_Count rms uncertainty on Count ct/s MaxLik Maximun likehood --- PPos Position probability % l_PCaII Limit flag on CaII --- PCaII CaII H&K probability number=3 Formal probability that if the star is responsible for the X-ray emission its chromospheric emission appears fainter or equal to the observed value. % tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Nov 18 Christian Motch <motch@cdsxb7.u-strasbg.fr> J_A+A_318_111.xml Planetary nebulae morphologies, central star masses and nebular properties J/A+A/318/256 J/A+A/318/256 Planetary nebulae properties Planetary nebulae morphologies, central star masses and nebular properties S K Gorny G Stasinska R Tylenda Astron. Astrophys. 318 256 1997 1997A&A...318..256G J/A+A/327/736 : Planetary nebulae properties (Stasinska+ 1997) Abundances Morphology Planetary nebulae planetary nebulae: general stars: AGB and post-AGB stars: fundamental parameters We have constituted a sample of about 80 PN with defined morphologies and well observed basic parameters (fluxes, angular radii, expansion velocities and magnitudes of the central stars). For these PN, we have derived the central star masses by comparing the observed set of parameters with those predicted by a simple evolutionary model of a PN, expanding at the same velocity as the observed one . We have then examined the relations between the PN morphological types and other properties, linked to the central star mass. Bipolar PN are shown to have a wider distribution of central star masses than the rest of PN, and shifted towards higher values. They lie closer to the Galactic plane and tend to have larger N/O ratios. Point symmetric PN, which have not been much studied so far, are found to constitute an outstanding class. They show an almost perfect M_*_-v_exp_ correlation. They correspond to a rather short evolutionary stage of PN. They lie, on average, further from the Galactic plane than bipolar PN and tend to have lower N/O. Globally, PN with higher central star masses are found closer to the Galactic plane, and the observed relation between N/O and M_*_ is roughly consistent with the predictions from evolutionary models for AGB stars.
Planetary nebulae properties and derived central stars masses, evolutionary ages and distances PNG PNG designation --- Name Other Name --- MType Morphological type number=1 Morphological type description: e, E, EH: elliptical nebulae B, BE: bipolar nebulae P, PE: point symmetric nebulae I: irregular nebulae --- u_MType Uncertainty flag on morphological type --- log(THI) Logarithm of HI Zanstra temperature K log(LHI) Logarithm of HI Zanstra luminosity solLum MagVis Absolute visual magnitude of the central star mag log(Rad) Logarithm of nebular radius pc log(SuBr) Logarithm of nebular surface brightness in H_beta mW/m2/sr log(Sv) Logarithm of S_v parameter mW/m2/sr DistS Shklovsky distance kpc l_Mass Lower limit flag on central star's mass --- Mass Derived mass of the central star solMass MassUp Upper limit to the central star's mass (where existing, individual cases only) solMass Age Derived evolutionary age 10+3yr Dist Derived distance kpc Chemical abundances of planetary nebulae PNG PNG designation --- Name Name --- MType Morphological type number=1 Morphological type description: e, E, EH: elliptical nebulae B, BE: bipolar nebulae P, PE: point symmetric nebulae I: irregular nebulae --- u_MType Uncertainty flag on morphological type --- a(N/H) Nitrogen abundance in respect to hydrogen log(N/H) + 12 --- r_a(N/H) References for N/H abundance number=2 This table is based on the references from Maciel & Koppen (1994A&A...282..436M) with the following updates: ASHAW84 - Adams et al., 1984MNRAS.207..471A CPT87 - Clegg et al., 1987MNRAS.224..761C CCMF96 - Costa et al., 1996A&AS..116..249C CFM93 - Costa et al., 1993A&A...276..184C CAK96 - Cuisinier et al., 1996A&A...307..215C KB94 - Kingsburgh & Barlow, 1994MNRAS.271..257K WBC93 - Walton et al., 1993IAUS..155..581W P91 - Perinotto, 1991ApJS...76..687P PRMG89 - Pena et al., 1989RMxAA..17...25P PRTM90 - Pena et al., 1990A&A...237..454P PTPD93 - Pena et al., 1993RMxAA..27..175P R91 - Ratag, 1991, thesis, University of Groningen TP79 - Torres-Peimbert & Peimbert, 1979RMxAA...4..341T --- a(O/H) Oxygen abundance in respect to hydrogen log(O/H) + 12 --- r_a(O/H) References for O/H abundance number=2 This table is based on the references from Maciel & Koppen (1994A&A...282..436M) with the following updates: ASHAW84 - Adams et al., 1984MNRAS.207..471A CPT87 - Clegg et al., 1987MNRAS.224..761C CCMF96 - Costa et al., 1996A&AS..116..249C CFM93 - Costa et al., 1993A&A...276..184C CAK96 - Cuisinier et al., 1996A&A...307..215C KB94 - Kingsburgh & Barlow, 1994MNRAS.271..257K WBC93 - Walton et al., 1993IAUS..155..581W P91 - Perinotto, 1991ApJS...76..687P PRMG89 - Pena et al., 1989RMxAA..17...25P PRTM90 - Pena et al., 1990A&A...237..454P PTPD93 - Pena et al., 1993RMxAA..27..175P R91 - Ratag, 1991, thesis, University of Groningen TP79 - Torres-Peimbert & Peimbert, 1979RMxAA...4..341T --- Patricia Bauer CDS 1996 Aug 12 J_A+A_318_256.xml The shape of the ionizing UV background at z~3.7 from the metal absorption systems of Q 0000-2619 J/A+A/318/347 J/A+A/318/347 Absorption lines in QSO 0000-2619 The shape of the ionizing UV background at z~3.7 from the metal absorption systems of Q 0000-2619 S Savaglio S Cristiani S D'Odorico A Fontana E Giallongo P Molaro Astron. Astrophys. 318 347 1997 1997A&A...318..347S QSOs Spectra, ultraviolet galaxies: formation intergalactic medium quasars: absorption lines quasars: individual (Q0000-2619) We give the list of absorption lines in the high resolution (FWHM=13 km/s) spectrum of the z=4.12 QSO 0000-2619. The first table contains the lines of the Lyman-alpha forest, while in the second table the lines of the metal systems are listed.
QSO 0000-2619 00 02 33.6 -26 02 18
Absorption line parameters of the Lyman-alpha forest Absorption line parameters of the metal systems No Line number --- lambda Line position 0.1nm logN HI column density [cm-2] e_logN rms uncertainty on logN [cm-2] b Doppler width km/s e_b rms uncertainty on b km/s z Redsfhit --- ID Line identification --- Note Note number=1 Lines marked with an asterisk have been fitted using simultaneously the observed Lyman-alpha and Lyman-beta profile. --- table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 Sandra Savaglio ESO Patricia Bauer CDS 1996 Jul 12 J_A+A_318_347.xml Rotation of the outer disc from classical Cepheids. J/A+A/318/416 J/A+A/318/416 Radial velocities & photometry of classical Cepheids Rotation of the outer disc from classical Cepheids. F Pont D Queloz P Bratschi M Mayor Astron. Astrophys. 318 416 1997 1997A&A...318..416P Photometry Radial velocities Stars, variable Cepheids Galaxy: kinematics and dynamics stars: distances Radial velocities and distances have been measured for a sample of 48 remote classical Cepheids located in the outer disc of the Galaxy (118deg<l<274deg). The distances are determined from BVI photometry, with semi-empirical metallicity corrections calibrated on the Magellanic Clouds. Using these Cepheids as tracers, the rotation curve of the disc is determined between R_0_ and 2R_0_. The result is a flat rotation curve about 30km/s lower than theta_0_, V_rot_=193+/-4km/s for R_0_==8.5kpc and theta_0_=220kms/s assumed, or V_rot_=167+/-4km/s for R_0_=8kpc and theta_0_=200km/s. The possible presence of non-axisymmetric components in the rotation of the outer disc is considered. We find a very small or vanishing value for any radial motion of the LSR or expansion/contraction motion.
Coravel measurements HJD Heliocentric Julian date d RV Radial velocity km/s e_RV rms uncertainty on RV km/s Name Object name --- Com Comment number=1 a: uncertain cross-correlation function b: doubtful identification c: almost certainly mistaken identification --- Elodie measurements HJD Heliocetric Julian date d RV Radial velocity km/s e_RV rms uncertainty in RV (photon noise only) km/s Name Object name --- Photometric measurements Name Object name --- HJD Heliocentric Julian date d Vmag V (Geneva) filter mag V-B V-B (Geneva) filter mag V-R V-R (Gunn) filter mag V-I V-I (Cousins) filer mag Com Comment number=1 a: low number of counts on B, uncertainty larger than 3% b: low number of counts on V c: observing run with too little standards observed, values with higher errors. --- Patricia Bauer CDS 1996 Jun 28 J_A+A_318_416.xml Is the symbiotic binary EG And an eclipsing system? J/A+A/318/53 J/A+A/318/53 UBV photometry of EG And Is the symbiotic binary EG And an eclipsing system? A Skopal Astron. Astrophys. 318 53 1997 1997A&A...318...53S Photometry, UBV Stars, variable binaries: symbiotic stars: individual (EG And) We present all available UBV photometry of the symbiotic binary EG And obtained during the last 10 years. The light curves display a double wave through one orbital cycle. It is shown that this behaviour cannot be explained by eclipses of the two detached sources of the continuum radiation. The present models of EG And are not able to simulate satisfactorily variation in both the far ultraviolet and the optical continuum.
EG And 00 44 37 +40 40 46
UBV observations of EG And HJD Heliocentric Julian day d DU U differential magnitude mag DB B differential magnitude mag DV V differential magnitude mag Ref References number=1 1 - Luthard (1987) =1987IBVS.3075....1L 2 - Skopal et al. (1991) =1991A&A...245..531S 3 - Hric et al. (1991) =1991CoSka..21..303H 4 - Skopal et al. (1992) =1992CoSka..22..131S 5 - Hric et al. (1993) =1993CoSka..23...73H 6 - Hric et al. (1994) =1994CoSka..24...31H 7 - Skopal et al. (1995) =1995CoSka..25...53S 8 - this paper --- Obs Observatory number=2 A - private station in Zweikirchen, B - Observatory of Brno C - Catania K - Kryonerion S - Soneberg SL - Stara Lesna W - Wroclaw SP - Skalnate Pleso --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 Jun 07 J_A+A_318_53.xml A general and practical method for calculating cosmological distances J/A+A/318/680 J/A+A/318/680 Cosmological distances A general and practical method for calculating cosmological distances R Kayser P Helbig T Schramm Astron. Astrophys. 318 680 1997 1997A&A...318..680K Gravitational lensing cosmology: miscellaneous cosmology: theory distance scale gravitational lensing methods: numerical The calculation of distances is of fundamental importance in extragalactic astronomy and cosmology. However, no practical implementation for the general case has previously been available. We derive a second-order differential equation for the angular size distance valid not only in all homogeneous Friedmann-Lemaitre cosmological models, parametrised by {lambda}_0_ and {OMEGA}_0_, but also in inhomogeneous `on-average' Friedmann-Lemaitre models, where the inhomogeneity is given by the (in the general case redshift-dependent) parameter {eta}. Since most other cosmological distances can be obtained trivially from the angular size distance, and since the differential equation can be efficiently solved numerically, this offers for the first time a practical method for calculating distances in a large class of cosmological models. We also briefly discuss our numerical implementation, which is publicly available.
angsiz.tex LaTeX version of the Appendix Patricia Bauer CDS 1996 May 06 Phillip Helbig <st2f304@hsvax1.hs.uni-hamburg.de> J_A+A_318_680.xml Cepheid radii and the CORS method revisited J/A+A/318/797 J/A+A/318/797 Cepheid radii Cepheid radii and the CORS method revisited V Ripepi F Barone L Milano G Russo Astron. Astrophys. 318 797 1997 1997A&A...318..797R Stars, diameters Stars, variable Cepheids stars: distances stars: fundamental parameters stars: oscillations We have refined the CORS method, introduced in 1980 for the computation of the Cepheid radii, in order to extend its applicability to recent and extensive sets of observations. The refinement is based on the computation, from observational data only, of one of the terms of the solving equation, previously based only on precise calibrations of photometric colors. A limited number of assumptions, generally accepted in the literature, is used. New radii are computed for about 70 Cepheids, and the resulting P-R relation is discussed.
Radii of Galactic Cepheids Name Name of the Cepheid --- Per Period of the Cepheid d rPhot Source of Photometry number=1 MB : BVR Photometry from Moffett and Barnes (1980ApJS...44..427M and 1984ApJS...55..389M) BMS : radial velocities from Barnes et al. (1987ApJS...65..307B and 1988ApJS...66...43B) WCBCM: radial velocities from Wilson et al. (1989ApJS...69..951W) BBB : Geneva System Photometry from Bersier et al. (1994, Cat. <J/A+AS/108/9>) BBMD : CORAVEL radial velocities from Bersier et al. (1994, Cat. <J/A+AS/108/25>) B : BVR Photometry from Berdnikov (1992A&AT....2....1B, 1992A&AT....2...47B and 1992A&AT....2..107B) M : BV Photometry from Madore (1995ApJS...29..219M) --- rRV Source of Radial Vel. number=1 MB : BVR Photometry from Moffett and Barnes (1980ApJS...44..427M and 1984ApJS...55..389M) BMS : radial velocities from Barnes et al. (1987ApJS...65..307B and 1988ApJS...66...43B) WCBCM: radial velocities from Wilson et al. (1989ApJS...69..951W) BBB : Geneva System Photometry from Bersier et al. (1994, Cat. <J/A+AS/108/9>) BBMD : CORAVEL radial velocities from Bersier et al. (1994, Cat. <J/A+AS/108/25>) B : BVR Photometry from Berdnikov (1992A&AT....2....1B, 1992A&AT....2...47B and 1992A&AT....2..107B) M : BV Photometry from Madore (1995ApJS...29..219M) --- RadSuBr Surface brightness radius number=2 Radius from Gieren W.P. et al. (1989ApJ...342..467G) solRad RadCORSo Radii obtained with "old" CORS solRad RadCORSn Radii obtained with the new CORS solRad Patricia Bauer CDS 1996 Jun 03 Vincenzo Ripepi <vincenzo@astr1pi.difi.unipi.it> J_A+A_318_797.xml Radiation transfer in circumstellar disks J/A+A/318/879 J/A+A/318/879 IR photometry of L1551/IRS5 Radiation transfer in circumstellar disks A B Men'shchikov T Henning Astron. Astrophys. 318 879 1997 1997A&A...318..879M Interstellar medium Photometry, infrared circumstellar matter methods: numerical radiative transfer stars: individual (L1551 IRS 5) We describe a new approach to the solution of the frequency-dependent stationary radiative transfer equation for axially-symmetric circumstellar dust disks. The method is applied to flared disks which are considered here as spheres with the polar cones removed. We have simplified the problem by computing the moments of the specific intensity only for the midplane and the surface of the flared disk. At the same time, we solve the radiative transfer equation exactly for an "equivalent" spherical envelope. The basic assumption is that density distribution in the disk depends only on the radial distance from the central star. This results in significantly faster calculations, reduces necessary computer memory, and allows incorporation of the algorithm into a hydrodynamical code. We applied our fast 2D radiative transfer code to a detailed modeling of the deeply embedded young stellar object (YSO) L1551 IRS 5. This is a YSO in the Taurus-Aurigae star-forming region, which has been very well studied with good spatial resolution and photometric data over the wide range from ultraviolet to millimeter wavelengths. Exploring the parameter space of our axially-symmetric models, we have found a self-consistent solution for L1551 IRS 5 explaining all available infrared and submm/mm continuum observations. Here, Appendices A, B, and C are presented, which are not available in the journal version of the paper. In Appendices A and B, one can find more details on the method and the overall iterative numerical scheme. Appendix C (Table C1) lists all published photometric observations of L1551 IRS 5, which we have found in the literature and which have been used in our modeling.
LDN 1551 IRS 5 IRAS 04287+1801 04 31 33.5 +18 08 15
Photometry of L1551 IRS 5 (from Appendix C) lambda Wavelength of observations um flux Observed flux Jy e_flux Flux uncertainty number=1 In few cases, when observers gave no information on accuracy of the measurements, the flux uncertainty is set to 0. Jy AppFlux Aperture (beam size FWHM) arcsec r_flux Abbreviated bibliographic reference --- Ref Full bibliographic reference --- appena.tex Details of the method appenb.tex Iterative scheme appenc.tex Photometry of L1551 IRS 5 Alexander Men'shchikov MPG AG "Staub...", Jena 1996 May 20 Alexander Men'shchikov <sascha@astro.uni-jena.de> J_A+A_318_879.xml A study of the Chamaeleon star forming region from the ROSAT all-sky survey: II. The pre-main sequence population. J/A+A/319/184 J/A+A/319/184 New WTTS in the Chamaeleon complex A study of the Chamaeleon star forming region from the ROSAT all-sky survey: II. The pre-main sequence population. J M Alcala J Krautter E Covino R Neuhaeuser J H M M Schmitt R Wichmann Astron. Astrophys. 319 184 1997 1997A&A...319..184A Stars, pre-main sequence ISM: individual (Chamaeleon clouds) stars: activity stars: pre-main sequence surveys X-rays: stars We analyse the nature of the optical counterparts of the ROSAT all-sky survey (RASS) X-ray sources identified with new weak-line T Tauri (WTTS) stars in the Chamaeleon star forming region (SFR). The new WTTS are distributed throughout the whole SFR, while the classical T Tauri stars (CTTS) are found only in the cloud cores. Adopting a distance of 150pc we derive the stellar parameters and place the new WTTS in the HR diagram. By comparison with theoretical pre-main sequence (PMS) evolutionary tracks, we find masses in the range of 0.2-2.5M_{sun}_ and ages from a few 10^5^yr to 5x10^7^yr. Many of the youngest WTTS are located far away from the main Chamaeleon dark clouds.
ROSAT
Stellar parameters of the new weak-line T Tauri stars (WTTS) in the Chamaeleon complex. RXJ ROSAT all-sky survey source designation Alcala' et al. (1995A&AS..114..109A) --- SpT Spectral type --- logTeff Logarithm of effective temperature K Av Visual stellar extinction mag Lbol Bolometric luminosity solLum Rad Stellar radius Sun RadBE Stellar radius derived from the Barnes-Evans relation Barnes & Evans (1976MNRAS.174..489B) Sun Mass Stellar mass number=1 Data derived using the pre-main sequence evolutionary tracks by D'Antona & Mazzitelli (1994ApJS...90..467D). solMass e_Mass Error on the stellar mass. solMass t Stellar age number=1 Data derived using the pre-main sequence evolutionary tracks by D'Antona & Mazzitelli (1994ApJS...90..467D). Myr e_t Error on the stellar age. Myr FHa H-alpha surface flux mW/m2 notes Notes to table number=2 a) stars lacking RI and JHKLM magnitudes. The luminosity for these stars was derived using UBV photometry and adopting a bolometric correction. b) visual binaries found by Brandner et al. (1996A&A...307..121B). c) designation by Walter (1992AJ....104..758W). d) designation by Lawson, et al. (1996MNRAS.280.1071L). e) probable spectroscopic binary (Covino et al. 1997). f) stars falling below the main sequence when adopting a distance of 150pc. --- X-ray data of the new WTTS in the Chamaeleon complex. RXJ ROSAT all-sky survey source designation Alcala' et al. (1995A&AS..114..109A) number=1 \d: X-ray fits with both NH and Tx as free parameters --- HR1 Hardness ratio 1 --- e_HR1 Error on hardness ratio 1 --- HR2 Hardness ratio 2 --- e_HR2 Error on hardness ratio 2 --- logNH Logarithm of Hydrogen column density cm-2 kTx X-ray emission energy keV e_kTx Error on X-ray emission energy keV ECF Energy conversion factor 10-18J/ct e_ECF Error on the energy conversion factor 10-18J/ct l_ECF Limit flag on ECF --- logLx Logarithm of the X-ray luminosity 10-7J e_logLx Error on logarithm of the X-ray luminosity 10-7J l_logFx Limit flag on logFx --- logFx Logarithm of the X-ray surface flux mW/m2 e_logFx Error on log. of the X-ray surface flux mW/m2 Patricia Bauer CDS 1996 Aug 12 Juan M. Alcala <jmae@rosat.mpe-garching.mpg.de> J_A+A_319_184.xml X-ray sources <1 degree from Seyfert galaxies. J/A+A/319/18 J/A+A/319/18 X-ray sources <1 degree from Seyfert galaxies X-ray sources <1 degree from Seyfert galaxies. H -D Radecke Astron. Astrophys. 319 18 1997 1997A&A...319...18R Galaxies, Seyfert X-ray source galaxies: Seyfert galaxies: spiral X-rays: galaxies Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (< about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04<B^o,i^_T_<12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.
ROSAT
Fields analyzed Object Object name (Seyfert galaxies and reference stars) used in the analysis --- Exp ROSAT PSPC exposure time ks GLAT Galactic latitude of the target object deg Bmag Brightness of the target object (Apparent blue magnitude, corrected for galactic and internal absorption) mag 1/2D25 Semi-apparent major isophotal diameter at surface brightness level 25.0 B-mag/arcsec^2^ arcmin Class Seyfert classification --- MType Seyfert type --- Detected Sources with counts rate above 5.0*10^-3^cts/s Field Field centered on the object mentioned --- Object Object number --- RAh Right ascension (2000) of the sources detected h RAm Right ascension (2000) of the sources detected min RAs Right ascension (2000) of the sources detected s DE- Declination sign --- DEd Declination (2000) of the sources detected deg DEm Declination (2000) of the sources detected arcmin DEs Declination (2000) of the sources detected arcsec PosOff Offaxis position of the detected sources arcmin Counts Rate Counts rate of the detected sources 10-3ct/s CF CF for control field --- Patricia Bauer CDS 1997 May 06 Hans Dieter Radecke <hdr@mpe-garching.mpg.de> J_A+A_319_18.xml A survey of CN in circumstellar envelopes J/A+A/319/235 J/A+A/319/235 CN in circumstellar envelopes survey A survey of CN in circumstellar envelopes R Bachiller A Fuente V Bujarrabal F Colomer C Loup A Omont T de Jong Astron. Astrophys. 319 235 1997 1997A&A...319..235B Abundances Stars, giant circumstellar matter molecular processes radio lines: stars stars: abundances stars: AGB and post-AGB We list in Table 1 the observed stars together with some of their characteristics. Distances, expansion velocities, mass loss rates, and spectral types are taken from the compilations of Bujarrabal et al. (1994) <J/A+A/285/247> and Loup et al. (1993A&AS...99..291). The sample includes C-rich and O-rich objects, some S-stars, a few proto-PN, and a young PN (NGC7027). See paper for more details. In Table 2, we give some of the observational parameters. A_low_ and A_high_ refer to the integrated intensity of the low-frequency and high-frequency fine-structure groups. The intrinsic intensity ratios, R=A_high_/A_low_, are R(1-0)=2 and R(2-1)=1.8. In principle, the observation of several components with different intrinsic strengths allows an estimate of the line optical depth, and the value of R gives an estimate of the envelope thickness.
Circumstellar envelopes observed in the CN lines Type C: C-rich object, O: O-rich object, blank: Other objects --- Name Star name --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Dist Distance kpc ExpV Expansion velocity km/s DMass Mass loss rate solMass/yr n_DMass Note on mass loss rate number=1 a: This value corresponds to the intense CO component which is superimposed on a broader emission plateau. --- Comment Spectral type and comments --- CN observational results Type C: C-rich object, O: O-rich object, blank: Other objects --- Name Source name --- l_Tpeak1 Limit flag on Tpeak1 --- Tpeak1 Peak temperature (N=1->0) K Ahigh1 Integrated intensity of the high-frequency fine-structure groups (N=1->0) K.km/s n_Ahigh1 Note on Ahigh1 number=1 b: From Bujarrabal & Cernicharo (1994A&A...288..551B) --- Alow1 Integrated intensity of the low-frequency fine-structure groups (N=1->0) K.km/s R1->0 Intensity ratio Ahigh1/Alow1 (N=1->0) number=3 The intrinsic intensity ratios, R=A_high_/A_low_, are R(1-0)=2 and R(2-1)=1.8. In principle, the observation of several components with different intrinsic strengths allows an estimate of the line optical depth, and the value of R gives an estimate of the envelope thickness --- e_Tpeak1 rms uncertainty on Tpeak1 (N=1->0) mK n_e_Tpeak1 Note on e_Tpeak1 number=2 a: Not observed in the 1-0 line --- Tpeak2 Peak temperature (N=2->1) K Ahigh2 Integrated intensity of the high-frequency fine-structure groups (N=2->1) K.km/s Alow2 Integrated intensity of the low-frequency fine-structure groups (N=2->1) K.km/s R2->1 Intensity ratio Ahigh2/Alow2 (N=2->1) number=3 The intrinsic intensity ratios, R=A_high_/A_low_, are R(1-0)=2 and R(2-1)=1.8. In principle, the observation of several components with different intrinsic strengths allows an estimate of the line optical depth, and the value of R gives an estimate of the envelope thickness --- e_Tpeak2 rms uncertainty on Tpeak2 (N=2->1) mK tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Aug 12 Rafael Bachiller <bachiller@conga.oan.es> J_A+A_319_235.xml The PAH hypothesis: a computational experiment on the combined effects of ionization and dehydrogenation on the IR signatures J/A+A/319/318 J/A+A/319/318 PAH hypothesis The PAH hypothesis: a computational experiment on the combined effects of ionization and dehydrogenation on the IR signatures F Pauzat D Talbi Y Ellinger Astron. Astrophys. 319 318 1997 1997A&A...319..318P Interstellar medium Spectra, infrared infrared: ISM: lines and bands ISM: molecules molecular data molecular processes IR spectra of anthracene and pyrene derivatives, serving as models for isolated, linear and isolated, compact PAHs, respectively, have been calculated using ab-initio quantum mechanical methods. The separate and combined effects of ionization and multiple dehydrogenation have been studied. This study confirms and refines the trends of our preliminary paper on the smallest possible PAH, naphthalene. If small PAHs are responsible for any UIR bands, they should be ionized and partially dehydrogenated, with a few triple bonds at the periphery of the carbon skeleton. In the appendix are given the complete IR spectra of all the isomers of the derivatives of anthracene and pyrene calculated for the purpose of this study. Tables I are for anthracene and Tables II for pyrene. Positions of the the missing hydrogens in the dehydrogenated species are referred as in Figures 1 and 2 of the original publication.
Computed IR spectra of neutral anthracene (1-2) doubly-dehydrogenated Anthracene IR spectra (2-3) doubly-dehydrogenated Anthracene IR spectra (1,2-3,4) quadri-dehydrogenated Anthracene IR spectra Computed IR spectra of neutral Pyrene (1-2) doubly-dehydrogenated Pyrene IR spectra (4-5) doubly-dehydrogenated Pyrene IR spectra (1,2-4,5) quadri-dehydrogenated Pyrene IR spectra (1,2-7,8) quadri-dehydrogenated Pyrene IR spectra (1,2-8,9) quadri-dehydrogenated Pyrene IR spectra (1,2-11,12) quadri-dehydrogenated Pyrene IR spectra (4,5-11,12) quadri-dehydrogenated Pyrene IR spectra Sym. Symmetry representation of the vibration --- Attrib. Assignment of the vibration number=1 r(CH) : CH bond stretching R(CC) : CC bond stretching a(CCC): CCC in-plane bending b(CH) : CH in-plane bending e(CH) : CH out-of-plane bending t(CCC): out-of-plane ring deformation --- nuN Neutral wave number cm-1 IntN Neutral intensity km/mol nuC Cation wave number cm-1 IntC Cation intensity km/mol Patricia Bauer CDS 1997 Feb 24 Yves Ellinger <ellinger@vega.ens.fr> J_A+A_319_318.xml Identification of X-ray sources <1{deg} from Seyfert galaxies. J/A+A/319/33 J/A+A/319/33 Identification of X-ray sources around Seyferts Identification of X-ray sources <1{deg} from Seyfert galaxies. H C Arp Astron. Astrophys. 319 33 1997 1997A&A...319...33A Galaxies, Seyfert X-ray sources BL Lacertae objects: general galaxies: Seyfert quasars: general X-rays: galaxies Excess numbers of X-ray sources around bright Seyfert galaxies have been demonstrated with significances of association up to 7.4-sigma (Radecke, 1997A&A...319...18R). The optical identification of these sources is shown here to be predominantly blue stellar objects (BSO's) of which some are already catalogued as quasars. Excluding the two brightest Seyferts, a subset of 24 with apparent magnitudes between 8.04<=B_T_^o,i^<=12.90mag. show a minimum excess of >46 bright X-ray sources. These excess X-ray sources are generally distributed between 10'<r<40' and 12 of the Seyferts show conspicuous pairs of X-ray sources across their active nuclei. Additional pairing and alignment of sources is seen for the remaining Seyferts. Among the paired X-ray sources, 53 have been identified as BSO's. Some double and multiple BSO's have been identified which are candidates for groups and associations of quasars. Some groups are well aligned and some centered on small blue galaxies. Four previously known BL Lac objects fall close enough to the Seyferts in this sample to confirm, at a significance level of 1-2x10^-9^, a previously reported association of BL Lac objects with bright, low redshift galaxies.
NGC 4235 12 17 09.8 +07 11 29 NGC 3516 11 06 47.4 +72 34 07 NGC 5273 13 42 08.3 +35 39 15 NGC 5548 14 17 59.5 +25 08 13
Position of optically identified X-ray Sources Gal Galaxy name --- C Counts of the source in the .5-20keV band number=1 Each map was inspected for patterns of pairs or alignments of sources across the central Seyfert. The sources which made up these patterns were then identified by their C=cts/ks values and are referred to by these numbers. ct/ks m_C Multiplicity index no C --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s u_RAs Uncertainty flag on right ascension --- DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec u_DEs Uncertainty flag on declination --- n_Emag B when Emag is Bmag --- l_Emag Limit flag on Emag --- Emag E magnitude or B magnitude if n_Emag = B mag l_O-E Limit flag on O-E --- O-E O-E color index mag n_O-E b for blue --- Ident Identification --- DELTAx X optical identification position with respect to the X-ray position number=2 + is East and - is West of the X-ray position + is North and - is South of the X-ray position arcsec DELTAy Y optical identification position with respect to the X-ray position number=2 + is East and - is West of the X-ray position + is North and - is South of the X-ray position arcsec Rem Remarks --- table3.tex TeX version of table3 Patricia Bauer CDS 1997 Feb 24 J_A+A_319_33.xml An HI survey of polar ring galaxies. II. The Effelsberg sample. J/A+A/319/401 J/A+A/319/401 HI survey of polar ring galaxies. II. An HI survey of polar ring galaxies. II. The Effelsberg sample. W K Huchtmeier Astron. Astrophys. 319 401 1997 1997A&A...319..401H Galaxies, ring H I data Radial velocities galaxies: distances and redshifts galaxies: elliptical and lenticular, cD galaxies: ISM radio lines: galaxies We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.
Optical and HI data PRC PRC identifier (=1990AJ....100.1489W) --- Name Galaxy name --- MType Morphological type --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEg Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec HRV Heliocentric optical radial velocity km/s e_HRV rms uncertainty on HRV km/s BT Total blue apparent magnitude mag D25 Major axis diameter arcmin SHI HI-flux Jy.km/s SMax Maximum intensity mJy e_SMax rms uncertainty on SMax mJy VHI HI-velocity km/s e_VHI rms uncertainty on VHI km/s dv20 linewidth at 20% of the peak km/s Derived global parameters from the combined sample of paper 1 and 2 PRC PRC identifier (=1990AJ....100.1489W) --- Name Galaxy name --- MType Morphological type --- LB B Luminosity 10+9solLum l_MHI Limit flag on MHI --- MHI HI mass 10+9solMass l_MHI/LB Limit flag on MHI/LB --- MHI/LB HI mass versus B luminosity ratio --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Feb 26 Walter Huchtmeier <p083huc@mpifr-bonn.mpg.de> J_A+A_319_401.xml Broad-band energy distribution of ROSAT detected quasars. I. Radio-loud objects. J/A+A/319/413 J/A+A/319/413 ROSAT detected quasars. I. Broad-band energy distribution of ROSAT detected quasars. I. Radio-loud objects. W Brinkmann W Yuan J Siebert Astron. Astrophys. 319 413 1997 1997A&A...319..413B VII/188 : Quasars and Active Galactic Nuclei (7th Ed.) (Veron+ 1996) IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) IX/11 : ROSAT Source Catalog (Voges+ 1994) Brinkmann W, Siebert J., 1995, A&A, 300, L33 =1995A&A...300L..33B Brunner H. et al., 1994, A&A 287, 436 =1994A&A...287..436B Buehler P. et al., 1995, A&A 295, 309 =1995A&A...295..309B Elvis M. et al., 1994, ApJ 422, 60 =1994ApJ...422...60E Laor A. et al., 1994, ApJ 435, 611 =1994ApJ...435..611L Neumann M. et al., 1994, A&AS 106, 303 =Cat. <J/A+AS/106/303> Schartel N. et al., 1996, A&A 307, 33 =1996A&A...307...33 Siebert J. et al., 1996, A&A 307, 8 =1996A&A...307....8S Veron-Cetty, M.-P. & Veron, P., 1993 (VV93) =Catalogue <VII/166> Voges W., 1992, In: Proc. of the ISY Conference ''Space Science'', ESA ISY-3, ESA Publications, p.9 (See catalogue <IX/10>) Voges W., et al., 1995, ROSAT NEWS No. 32 =Catalogue <IX/11> Zhang Y. F., Marscher A. P., 1994, AIP Conf. Proc. 313, p.406 QSOs X-ray sources galaxies: active quasars: general radio lines: galaxies X-rays: galaxies We have compiled a sample of all quasars with measured radio emission from the Veron-Cetty - Veron catalogue (1993, VV93 <VII/166>) detected by ROSAT in the ALL-SKY SURVEY (RASS, Voges 1992), as targets of pointed observations, or as serendipitous sources from pointed observations as publicly available from the ROSAT point source catalogue (ROSAT-SRC, Voges et al. 1995). The total number of ROSAT detected radio quasars from the above three sources is 654 objects. 69 of the objects are classified as radio-quiet using the defining line at a radio-loudness of 1.0, and 10 objects have no classification. The 5GHz data are from the 87GB radio survey, the NED database, or from the Veron-Cetty - Veron catalogue. The power law indices and their errors are estimated from the two hardness ratios given by the SASS assuming Galactic absorption. The X-ray flux densities in the ROSAT band (0.1-2.4keV) are calculated from the count rates using the energy to counts conversion factor for power law spectra and Galactic absorption. For the photon index we use the value obtained for a individual source if the estimated 1 sigma error is smaller than 0.5, otherwise we use the mean value 2.14.
ROSAT
654 ROSAT detected radio quasars IAU IAU name of the object --- n_IAU A flag for classification --- Name Alternative name from VV93 <VII/166> A '*' denotes a radio-quiet object; a '?' mark indicates that no 5GHz flux is available; and a '!' means that the X-ray flux is probably corrupted by another source. --- RAh Right ascension J2000 (hours) h RAm Right ascension J2000 (minutes) min RAs Right ascension J2000 (seconds) s DE- Declination sign --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (') arcmin DEs Declination J2000 (") arcsec z Redshift A '0' as the 3rd decimal is mostly an artifact of the machine readable form of the catalogue. See the printed version of VV93 <VII/166> for the appropriate values. --- Vmag Magnitude from VV93 <VII/166> One sigma statistical errors from count rates only mag F6cm 6cm radio flux density Jy alpha_r Radio spectral index --- Fx Unabsorbed X-ray flux density 10-12mW/m2 e_Fx Error of X-ray flux density 10-12mW/m2 Gamma X-ray spectral photon index Spectral photon index in the ROSAT energy band for a power law fit (S=C*E**(-Gamma)) with Galactic absorption --- E_Gamma Positive error of photon index One sigma errors. If no error is given, the value of the error is unphysically large. --- e_Gamma Negative error of photon index --- Com Notes on the X-ray detection S: detected in RASS; P: detected in Pointed observations --- Ref Reference for the quoted spectral index BP: Buehler P., et al. (1995A&A...295..309B) BH: Brunner H., et al. (1994A&A...287..436B) BW: Brinkmann W. & Siebert J. (1995A&A...300L..33B) EM: Elvis M., et al. (1994ApJ...422...60E) LA: Laor A., et al. (1994ApJ...435..611L) NM: Neumann M., et al. <J/A+AS/106/303> SN: Schartel N., et al. (1996A&A...307...33) SJ: Siebert J., et al., (1996A&A...307....8S) ZY: Zhang Y.F. & Marscher A.P., 1994 AIP Conf. Proc. 313, p.406 --- Patricia Bauer CDS 1996 Sep 27 Weimin Yuan <wey@ipp-garching.mpg.de> J_A+A_319_413.xml Red giants in open clusters. VI. Orbits of ten spectroscopic binaries. J/A+A/319/481 J/A+A/319/481 Radial velocities of 10 spectroscopic binaries Red giants in open clusters. VI. Orbits of ten spectroscopic binaries. J -C Mermilliod J Andersen M Mayor Astron. Astrophys. 319 481 1997 1997A&A...319..481M Binaries, spectroscopic Clusters, open Radial velocities binaries: spectroscopic open clusters and associations: general stars: fundamental parameters We present new orbits for ten (single-lined) spectroscopic binaries in seven open clusters: NGC 2489, 2567, 3033, 5822, 6134, 6664 and IC 2488 based on 243 individual radial velocities obtained with the southern CORAVEL scanner. The orbital periods range from 98.5 to 3566 days. The shortest-period orbit is circular, as expected. Seven of the binaries are confirmed cluster members, one is a possible member, and two are clearly non-members. Maximum masses from photometric separation and minimum masses from the spectroscopic orbits define the mass of the secondaries within an interval of M_max_-M_min_=0.5M_{sun}_. NGC 6664 #54 seems to have a rather massive secondary (M>3M_{sun}_), but the UBV colours appear normal for a luminous red giant, while significantly bluer (B-V) and (U-B) colours would be expected. It could be a triple system, the secondary being itself a short period binary. This paper brings the number of orbits published in this programme to 53, 45 of which are confirmed red-giant cluster members and 8 are non-members
NGC 2489 C 0754-299 (#25) 07 56.2 -30 04 NGC 2567 C 0816-304 (#104) 08 18.4 -30 39 NGC 3033 C 0947-561 (#12, #19) 09 48.8 -56 25 NGC 5822 C 1501-541 (#3, #312) 15 05.2 -54 21 NGC 6134 C 1624-490 (#8, #34) 16 27.7 -49 09 NGC 6664 C 1834-082 (#54) 18 36.7 -08 13 IC 2488 C 0926-567 (#128) 09 27.6 -56 59
Radial velocity data LID Cluster - Star number number=1 The numbering systems used are from: NGC 2489 Lindoff U., Johansson K. 1968, Ark. Astr 5, 45 (1968ArA.....5...45L) NGC 2567 Lindoff U. 1968, Ark. Astr 4, 587 (1968ArA.....4..587) NGC 3033 Vogt N., Moffat A.F.J. 1972, A&A 9, 97 (1973A&AS....9...97V) NGC 5822 Bozkurt S. 1974, Rev. Mex. A.A. 1, 89 (1974RMxAA...1...89B) NGC 6134 Lindoff U. 1972, A&AS 7, 231 (1972A&AS....7..231L) NGC 6664 Arp H.C. 1958, ApJ 128, 166 (1958ApJ...128..166A) IC 2488 Pedreros M. 1987, AJ 94, 92 (1987AJ.....94...92P) LID: NGC clusters: 2nnnnssss nnnn = NGC number, ssss = star number IC clusters: 3iiiissss iiii = IC number, ssss = star number --- HJD Heliocentric Julian Date d RV Radial velocity km/s e_RV Error on the radial velocity km/s Patricia Bauer CDS 1996 Aug 12 Jean-Claude Mermilliod <Jean-Claude.Mermilliod@obs.unige.ch> J_A+A_319_481.xml New beryllium observations in low-metallicity stars J/A+A/319/593 J/A+A/319/593 [Be] abundances in low-metallicity stars New beryllium observations in low-metallicity stars P Molaro P Bonifacio F Castelli L Pasquini Astron. Astrophys. 319 593 1997 1997A&A...319..593M Abundances Stars, metal-deficient cosmic rays cosmology: observations Galaxy: evolution stars: abundances stars: Population II We present observations of the Be II 313.0nm resonance doublet in 14 halo and old disk stars with metallicities ranging from [Fe/H]=-0.4 to =~-3.0 obtained with the CASPEC spectrograph of the ESO 3.6m telescope at a FWHM=~8.6km/s resolution. Abundances are derived by means of the synthetic spectra technique employing Kurucz (1993, CD-ROM 13 and CD-ROM 18) atmospheric models, with enhanced {alpha}-elements and no overshooting.
Errors in logg HD HD number --- Teff Effective temperature K [Fe/H] Metallicity --- logg Surface gravity cm/s2 Dphot rms uncertainty on logg due to random errors in the photometry cm/s2 Dred rms uncertainty on logg due to reddening cm/s2 DTeff rms uncertainty on logg due to Teff cm/s2 D[Fe/H] rms uncertainty on logg due to metallicity cm/s2 Dlogg rms uncertainty on surface gravity calculated as the square root of the sum of the squares of these four uncertainties cm/s2 Errors on Be abundances HD HD number --- Dg Error in [Be] due to logg Sun DTeff Error in [Be] due to effective temperature Sun D[Fe/H] Error in [Be] due to metallicity Sun D[Be]sys Total error on [Be] due to atmospheric parameters Sun D[Be]stat Error associated with the noise in the data Sun D[Be] Error on [Be] (D[Be]sys + D[Be]stat) Sun Abundance for BK halo stars HD HD number --- Teff Effective temperature K logg Surface gravity cm/s2 [Be] abundance Sun u_[Be] Uncertainty flag on [Be] --- [Fe/H] Metallicity Sun Be abundance for halo stars Name Star name --- Teff Effective temperature K logg Surface gravity cm/s2 [Fe/H] Metallicity Sun l_[Li] Limit flag on [Li] --- [Li] Li abundance Sun l_[Be] Limit flag on [Be] --- [Be] Be abundance Sun e_[Be] rms uncertainty on [Be] Sun ref References number=1 1: this paper 2: Garcia-Lopez et al. (1995A&A...302..184G) 3: Boesgaard & King (1993AJ....106.2309B) 4: Boesgaard & King revised (1993) 5: Ryan et al. (1991), (1992ApJ...388..184R) 6: Gilmore et al. (1992Natur.357..379G) 7: Rebolo et al. (1988A&A...193..193R) Li abundances are from Boesgaard & King (1993AJ....106.2309B), Molaro (1991MmSAI..62...17M), or from the literature as specified in the text. --- Patricia Bauer CDS 1996 Sep 02 J_A+A_319_593.xml HI observations of dwarf galaxies in voids J/A+A/319/67 J/A+A/319/67 HI observations of dwarf galaxies in voids HI observations of dwarf galaxies in voids W K Huchtmeier U Hopp B Kuhn Astron. Astrophys. 319 67 1997 1997A&A...319...67H Galaxies, optical H I data Magnitudes Redshifts cosmic rays cosmology: observations Galaxy: evolution stars: abundances stars: Population II We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2<=logL_B_<=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.
Optical data Name Galaxy name number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' --- RAh Optical right ascension (1950.0) number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' h RAm Optical right ascension (1950.0) number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' min RAs Optical right ascension (1950.0) number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' s DE- Declination sign number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' --- DEd Optical declination (1950.0) number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' deg DEm Optical declination (1950.0) number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' arcmin DEs Optical declination (1950.0) number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' arcsec mB Apparent blue magnitude number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' mag mR Apparent red magnitude number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' mag a25 Blue major axis at a surface brightness of 25 mag/arcsec^2 number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' arcsec b25 Blue minor axis at a surface brightness of 25 mag/arcsec^2 number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' arcsec z Redshift number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' --- e_z rms uncertainty on z number= CGCG0021+1358 - edge-on spiral of similar size at 3.9' O0823-055 - E-type galaxy at 5.2' CGCG1022-0036 - in group of four galaxies of similar size at 1.5', 4.6', and 6.9'; interaction with closest neighbour? O0467-106 - spiral of similar size at 3.5' O0467-023 - spiral of similar size at 3' O0467-009 - elliptical galaxy at 1.8', foreground? VN2#274 - VN2#K363 at 4.4', and a small (10") background spiral VN2#253 at 3.6' VN2#KOW363 - VN2#274 at 4.4' VN4#109 - CGCG1305+3421 (elliptical) at 2.6' VN4#080 - UGC8227 at 5.7' VN4#071 - nearby spiral VN#70 with different z (0.065) at 1.3' CGCG1305+3421 - VN4#109 at 2.6' CGCG1305+3416 - dE companion UGC8227 - VN4#080 at 5.7' , VN4#069 at 4.4' A2151-0033 - three spirals at 4.2', 4.9', and 6.4' A2151-0035 - A2151-0035 at 4.5', other spirals at 3.7', and 2.6' --- MClass Morphological classification number=1 Morphological classification deviates from the usual system : lsb marks a low-surface-brightness object, S marks a disk galaxy which can not be classified in more detail. ed is an edge-on disk. --- gd Parameter describing the galaxian density number=2 1 cluster; 2 sheet; 3 rim of sheet; 4 transition sheet-void; 5 rim of void; 6 void --- HI-observations of dwarf galaxies in voids ID Identification number --- Name Galaxy name --- Stot Total line flux Jy.km/s Smax Peak flux mJy e_Smax rms uncertainty on Smax mJy HRV HI-line heliocentric radial velocity number=1 Mean of the two midline velocities at a level of 25% and 20% of the peak. km/s e_HRV rms uncertainty on HRV km/s LW50 Observed line width at a level of 50% --- LW25 Observed line width at a level of 25% --- LW20 Observed line width at a level of 20% --- MHI Total HI-mass 10+9solMass MHI/LB MHI/LB ratio --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Feb 19 Walter Huchtmeier <p083huc@mpifr-bonn.mpg.de> J_A+A_319_67.xml Beamed radio and far infrared emission in quasars and radio galaxies J/A+A/319/757 J/A+A/319/757 Quasar and radio galaxies flux densities Beamed radio and far infrared emission in quasars and radio galaxies H Hoeksta P D Barthel R Hes Astron. Astrophys. 319 757 1997 1997A&A...319..757H Galaxies, radio QSOs galaxies: active galaxies: jets infrared: galaxies quasars: general The tables described below contain the data used in the analysis. The data have been taken from various sources in the literature. The references to the data can be found in the paper. Table 1 contains the data of the 3C radio galaxy sample. Table 2 contains the data of the 3C quasar sample. Table 3 contains the data of the 4C quasar sample. The tables list the name of the object, its redshift, the value of the Q-parameter (ratio between the core and extended flux at 5 GHz observed frequency), and the flux densities at various frequencies.
Data of 3C radio galaxy sample Data of 3C quasar sample Data of 4C quasar sample Name Name of the object --- z Redshift of the object --- log(Q) Q-parameter (ratio between the core and extended flux at 5 GHz observed frequency) --- F178MHz Flux density extended emission at 178 MHz Jy F318MHz Total flux density at 318 MHz Jy F408MHz Total flux density at 408 MHz Jy F750MHz Total flux density at 750 MHz Jy F1400MHz Total flux density at 1.4 GHz Jy F2700MHz Total flux density at 2.7 GHz Jy F5000MHz Total flux density at 5.0 GHz Jy F10700MHz Total flux density at 10.7 GHz Jy F14900MHz Total flux density at 14.9 GHz Jy F60um Total flux density at 60 micron mJy Patricia Bauer CDS 1996 Aug 23 Henk Hoekstra <hoekstra@astro.rug.nl> J_A+A_319_757.xml Search for forced oscillations in binaries. I. The eclipsing and spectroscopic binary V436 Persei = 1 Persei J/A+A/319/867 J/A+A/319/867 V436 Persei = 1 Persei byBV photometry Search for forced oscillations in binaries. I. The eclipsing and spectroscopic binary V436 Persei = 1 Persei P Harmanec P Hadrava S Yang D Holmgren P North P Koubsky J Kubat E Poretti Astron. Astrophys. 319 867 1997 1997A&A...319..867H Binaries, eclipsing Binaries, spectroscopic binaries: eclipsing binaries: spectroscopic stars: fundamental parameters stars: individual (V436 Per, 1 Per) stars: oscillations Outline of a project aimed at testing the presence of rapid line-profile variations in the atmospheres of hot components of close binaries is presented and its first results are described. An analysis of new electronic spectra of the eclipsing binary V436 Per from three observatories and of photoelectric observations, obtained earlier by several authors, leads to a unique determination of all basic physical elements of this interesting object. The first practical application of a new method of spectral disentangling allowed us to obtain, for the first time, individual accurate line profiles of both binary components and to derive their rotational velocities and orbital radial-velocity curves. We also detected absorption sub-features travelling from blue to red accross the He I 6678 line profile, in a series of six spectra taken during one night. At least one of the components of V436 Per is, therefore, a new hot line-profile variable.
V436 Per 1 Per HD 11241 HR 533 01 51 59.3 +55 08 51
V436 Per yellow photoelectric observations V436 Per blue photoelectric observations HJD Heliocentric Julian date d Color Color number=1 y, b : Stromgren y&b magnitudes V, B : Johnson V&B magnitudes VG, BG: Geneve V&B magnitudes --- Mag Measured V436 Per magnitude in color band mag w_Mag Weight assigned to individual data sets --- Code Numerical code identifying sources of data number=2 3: y (Stromgren) magnitude, Kurtz (1977PASP...89..939K) 4: V Geneve magnitude, North & Rufener (1981IBVS.2036....1N) 6: V Johnson magnitude, Poretti (1982IBVS.2129....1P) 7: V Johnson magnitude, Bohme (1984IBVS.2507....1B) 8: V Johnson magnitude, Poretti (1984IBVS.2529....1P) and this paper 11: B Johnson magnitude, Gussow (1929AN....237..321G) - observations relative to 4 Per 12: B Johnson magnitude, Gussow (1929AN....237..321G) - observations relative to 2 Per 14: B Geneve magnitude, North & Rufener (19811IBVS.2036....1N) 15: b Stromgren magnitude, Percy (1982IBVS.2085....1P) --- Patricia Bauer CDS 1996 Sep 03 Petr Harmanec <hec@sunstel.asu.cas.cz> or <hec@mbox.cesnet.cz> J_A+A_319_867.xml Absolute magnitudes and kinematics of barium stars J/A+A/319/881 J/A+A/319/881 Ba II strength of barium stars Absolute magnitudes and kinematics of barium stars A E Gomez X Luri S Grenier L Prevot M -O Mennessier F Figueras J Torra Astron. Astrophys. 319 881 1997 1997A&A...319..881G Stars, barium kinematics stars: absolute magnitudes stars: barium The absolute magnitude of barium stars has been obtained from kinematical data using a new algorithm based on the maximum-likelihood principle. The method allows to separate a sample into groups characterized by different mean absolute magnitudes, kinematics and z-scale heights. Three groups belonging to the disk population have been obtained. We give, for each star of these three groups, the probability P of belonging to each of them and the assignation to the most likely one (G). The first column gives an an identification number: for most of the stars HD numbers are given, otherwise BD numbers. The following two columns present the spectral type taken from the INCA database and the strength of the BaII line (I_Ba) taken from Lu catalogue (1991) <V/81>.
Probability assignation to groups HD/BD HD or BD number --- Sp Spectral Type --- BaClass Barium intensity class --- BaCode Barium intensity code number=1 c certain Ba stars in MacConnell, Frye, Upgren (1972AJ.....77..384M) m marginal Ba in MacConnell, Frye, Upgren (1972AJ.....77..384M) n non-barium stars (see Paper I, Lu et al. (1983AJ.....88.1367L)) s not explained by Lu in his paper : uncertainty flag on BaClass --- G Assigned Group --- P1 Probability of belonging to Group 1 number=2 Group 1: Bright G and K giants Group 2: Normal G and K giants Group 3: G-type subgiants % P2 Probability of belonging to Group 2 number=2 Group 1: Bright G and K giants Group 2: Normal G and K giants Group 3: G-type subgiants % P3 Probability of belonging to Group 3 number=2 Group 1: Bright G and K giants Group 2: Normal G and K giants Group 3: G-type subgiants % Patricia Bauer CDS 1996 Aug 28 Ana E. Gomez <Ana.Gomez@obspm.fr> J_A+A_319_881.xml The T Tauri star population in the Lupus star forming region J/A+A/320/185 J/A+A/320/185 UBVRIcJHKL photometry in Lup The T Tauri star population in the Lupus star forming region R Wichmann J Krautter E Covino J M Alcala R Neuhaeuser J H M M Schmitt Astron. Astrophys. 320 185 1997 1997A&A...320..185W Photometry, UBVRIJKLMNH Stars, pre-main sequence stars: formation stars: late-type stars: pre-main sequence X-rays: stars In a recent study, some 130 new weak-line T Tauri stars (WTTS) have been discovered in the Lupus star forming region (SFR). Some of these stars are seen projected onto regions of high obscuration, while others are located far from the Lupus dark clouds. In this paper we present photometric observations of a large sample of these WTTS. We estimate effective temperatures and luminosities for the stars observed, and derive masses and ages by comparison with theoretical evolutionary tracks. The mean age of WTTS seen in projection against the dark clouds is found to be lower than the mean age of WTTS discovered far from regions of high obscuration, and yet higher than the mean age of the classical T Tauri stars (CTTS) in Lupus. Moreover, while the CTTS in Lupus show an unusual predominance of very low-mass stars, the WTTS population in Lupus contains many stars with comparatively higher masses. Correlations between the X-ray emission and other stellar parameters, like bolometric luminosity, radius, mass, and age, are studied, and the results are discussed. For a description of the UBV, (RI)c and JHKL photometric systems, see e.g. <GCPD/01>, <GCPD/54> and <GCPD/09>
Photometry of Lupus T Tauri stars Star Identifier of star from ROSAT --- Vmag V magnitude mag B-V B-V color index mag U-B U-B color index mag V-Rc V-R(Cousin) color index mag V-Ic V-I(Cousin) color index mag Jmag J magnitude mag e_Jmag Error of J magnitude 0.01mag Hmag H magnitude mag e_Hmag Error of H magnitude 0.01mag Kmag K magnitude mag e_Kmag Error of K magnitude 0.01mag Lmag L magnitude mag e_Lmag Error of L magnitude 0.01mag Stellar properties of Lupus T Tauri stars Star Identifier of star --- SpType Spectral type --- Teff Effective temperature K log(L) Log(L_bol) solLum AV Extinction A(V) mag Rad Radius Sun Mass Mass number=1 Masses and ages are from evolutionary tracks by D'Antona and Mazzitelli (1994ApJS...90..467D) solMass l_log(age) Lower limit indicator number=2 U indicates that age is lower limit, otherwise blank --- log(age) Log(age) number=1 Masses and ages are from evolutionary tracks by D'Antona and Mazzitelli (1994ApJS...90..467D) yr D(H-K) Delta (H-K) mag Patricia Bauer CDS 1996 Oct 09 Rainer Wichmann <R.Wichmann@lsw.uni-heidelberg.de> J_A+A_320_185.xml Investigation of the Pleiades cluster. III. Additional corona members J/A+A/320/74 J/A+A/320/74 Radial velocities of Pleiades members Investigation of the Pleiades cluster. III. Additional corona members J -C Mermilliod P Bratschi P Mayor Astron. Astrophys. 320 74 1997 1997A&A...320...74M Radial velocities open clusters and associations: general open clusters and associations: individual (Pleiades) techniques: radial velocities The analysis of CORAVEL radial velocities of 93 stars selected on the basis of their proper motion and Geneva CCD photometric observations for 57 stars have permitted to identify 25 new members in the outer part of the Pleiades. Several spectroscopic binaries have been discovered, but their membership is not clear. Two orbits with short periods have been determined, but both stars are probably non-members. The total number of member stars in the outer part of the Pleiades in the spectral range F5-K0 (0.45<B-V<0.90) is now 81 which is comparable to the number of stars known in Hertzsprung's central area (88 stars) in the same spectral domain. Therefore at least 48% of the F5-K0 main-sequence stars are located in the outer part of the cluster. And the census is probably still incomplete.
Observational data for non-member stars AK Star number from Artjukhina and Kalinina (1970) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude (see text) mag [B-V] Geneva CCD [B-V] colour index mag B-V Johnson B-V colour index mag RV Mean radial velocity km/s e_RV Error on the radial velocity km/s N Number of RV observations --- DeltaT Time interval d P(chi2) Probability of non variability --- RVc Computed radial velocity km/s O-C Observed minus Computed km/s Prob Proper-motion membership probability --- Remark Remarks --- Patricia Bauer CDS 1996 Sep 03 Jean-Claude Mermilliod <Jean-Claude.Mermilliod@obs.unige.ch> J_A+A_320_74.xml The stellar population of the globular cluster M 3. II. CCD photometry of additional 10,000 stars J/A+A/320/757 J/A+A/320/757 M 3 stars CCD photometry The stellar population of the globular cluster M 3. II. CCD photometry of additional 10,000 stars F R Ferraro E Carretta C E Corsi F Fusi Pecci C Cacciari R Buonanno B Paltrinieri D Hamilton Astron. Astrophys. 320 757 1997 1997A&A...320..757F J/A+A/290/69 : M3 photographic photometry (Buonanno+, 1994) Clusters, globular Photometry, CCD globular clusters: individual (M 3) photometry, CCD stars: Population II We present BVI CCD photometry for more than 10,000 stars in the innermost region (0.3'<r<~4') of the globular cluster M 3. When added to the previous photographic photometry by Buonanno et al. (1994A&A...290...69B) reaching as far as r~7', this results in an homogeneous data-set including about 19,000 stars measured in this cluster, which can be now regarded as one of the main templates for stellar population studies.
M 3 NGC 5272 13 42.2 +28 23
V,B,I photometry of 20191 stars in M 3 Name Star designation (this paper) --- Vmag V magnitude mag Bmag B magnitude mag Imag I magnitude mag Xpos X coordinate (arcsec) arcsec Ypos Y coordinate (arcsec) arcsec Star Name of the stars (if variable) in the 3rd Sawyer-Hogg catalog (1973PDDO....3....6S) --- n_Star 0: constant stars, 1: variable stars --- Patricia Bauer CDS 1996 Nov 07 Eugenio <CARRETTA@astbo3.bo.astro.it> J_A+A_320_757.xml Tidal radii of the globular clusters M 5, M 12, M 13, M 15, M 53, NGC 5053 and NGC 5466 from automated star counts. J/A+A/320/776 J/A+A/320/776 Tidal radii of 7 globular clusters Tidal radii of the globular clusters M 5, M 12, M 13, M 15, M 53, NGC 5053 and NGC 5466 from automated star counts. I Lehmann R -D Scholz Astron. Astrophys. 320 776 1997 1997A&A...320..776L Clusters, globular globular clusters: general methods: statistical We present new tidal radii for seven Galactic globular clusters using the method of automated star counts on Schmidt plates of the Tautenburg, Palomar and UK telescopes. The plates were fully scanned with the APM system in Cambridge (UK). Special account was given to a reliable background subtraction and the correction of crowding effects in the central cluster region. For the latter we used a new kind of crowding correction based on a statistical approach to the distribution of stellar images and the luminosity function of the cluster stars in the uncrowded area. The star counts were correlated with surface brightness profiles of different authors to obtain complete projected density profiles of the globular clusters. Fitting an empirical density law (King 1962AJ.....67..471K) we derived the following structural parameters: tidal radius rt, core radius rc and concentration parameter c. In the cases of NGC 5466, M 5, M 12, M 13 and M 15 we found an indication for a tidal tail around these objects (cf. Grillmair et al., 1995AJ....109.2553G).
M 5 NGC 5904 C 1516+022 15 18 33.7 +02 04 58 M 12 NGC 6218 C 1644-018 16 47 14.4 -01 56 52 M 13 NGC 6205 C 1639+365 16 41 41.4 +36 27 37 M 15 NGC 7078 C 2127+119 21 29 58.3 +12 10 00 M 53 NGC 5024 C 1310+184 13 12 55.1 +18 12 09 NGC 5053 C 1313+179 13 16 26.9 +17 41 52 NGC 5466 C 1403+287 14 05 27.3 +28 32 04
Star count Name Galaxy name --- Rad Mean radius of an annulus arcmin Dens Background and crowding corrected stellar density in number per arcmin^2^ ct/arcmin2 e_Dens uncertainty in Dens (number per arcmin^2^) ct/arcmin2 Patricia Bauer CDS 1998 Feb 23 Ingo Lehmann <ilehmann@aip.de> J_A+A_320_776.xml Mass-luminosity relation of low-mass stars J/A+A/320/79 J/A+A/320/79 Mass-luminosity relation of low-mass stars Mass-luminosity relation of low-mass stars O Yu Malkov A E Piskunov D A Shpil'kina Astron. Astrophys. 320 79 1997 1997A&A...320...79M Stars, late-type Stars, masses stars: late-type stars: low-mass, brown dwarfs stars: luminosity function, mass function To construct the MLR, empirical data for 56 stars in 30 low mass multiple systems, main sequence components of spectral class M0 and later were collected and processed. We considered only those systems where the determination of dynamical masses of components is possible, that is, where masses are derived directly from celestial mechanical considerations rather than from relations between mass and some observational parameter.
Systems data GJ Gliese & Jahreiss (GJ) <V/70> nomenclature from Preliminary Version of the Third Catalogue of Nearby Stars. --- n_GJ a: systems that have no GJ names --- Plx Parallax arcsec e_Plx Parallax accuracy arcsec Per Period number=1 Data is present when used for the mass calculation, otherwise blank yr e_Per Period accuracy number=1 Data is present when used for the mass calculation, otherwise blank yr a Semimajor axis number=1 Data is present when used for the mass calculation, otherwise blank arcsec e_a Semimajor axis accuracy number=1 Data is present when used for the mass calculation, otherwise blank arcsec Mass Fractional mass of the secondary number=1 Data is present when used for the mass calculation, otherwise blank --- e_Mass Fractional mass accuracy number=1 Data is present when used for the mass calculation, otherwise blank --- Refs References detailed in file "refs.dat" --- Components data GJ Gliese & Jahreiss (GJ) <V/70> nomenclature from Preliminary Version of the Third Catalogue of Nearby Stars. --- n_GJ a: systems that have no GJ names --- Vmag Visual stellar magnitude mag e_Vmag Visual stellar magnitude accuracy mag flareFlag * indicating flare stars --- BolCorr Bolometric correction (if known) mag e_BolCorr Bolometric correction accuracy (if known) mag M(Vmag) Absolute stellar magnitude mag e_M(Vmag) Absolute stellar magnitude accuracy mag log(L) Bolometric luminosity (if known) [solLum] e_log(L) Bolometric luminosity accuracy (if known) [solLum] Mass Mass solMass e_Mass Mass accuracy solMass Note2 + indicating stars with the best data --- References of table2 RefNo Reference number --- --- Separator --- Text Name of author(s), and bibcode --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Oct 07 J_A+A_320_79.xml The optical variability of QSOs. II. The wavelength dependence J/A+A/321/123 J/A+A/321/123 Optical variability of QSOs The optical variability of QSOs. II. The wavelength dependence S Cristiani S Trentini F La Franca P Andreani Astron. Astrophys. 321 123 1997 1997A&A...321..123C QSOs quasars: general The SA94 variability sample is made up of 149 optically selected quasars listed in this table, observed in a rectangular area of the sky within the limits 2h 43m 51.2s < RA < 2h 59m 14.3s, -2deg 03' 23.8" < DEC < 2deg 32' 11.0" (Epoch 1950.0), covering 17.66 sq.deg.
List of the QSOs in the SA94 RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec z Redshift --- R' Magnitude R' mag IDX Variability index mag+2 Type See Note number=1 a: Cristiani S., La Franca F., Barbieri C., Clowes R.G., Iovino A., 1991MNRAS.250..531C b: Barbieri C., Cristiani S., 1986A&AS...63....1B c: Veron-Cetty M.P., Veron P., 1993, Catalogue <VII/18> d: La Franca F., Cristiani S., Barbieri C., 1992AJ....103.1062L e: Cristiani S., Trentini S., La Franca F., Aretxaga I., Andreani P., Vio R., Gemmo A., (Paper I) 1996A&A...306..395C --- Stefano Cristiani Universita` di Padova 1996 Oct 16 Stefano Cristiani <cristiani@astrpd.pd.astro.it> J_A+A_321_123.xml Interstellar extinction and the intrinsic spectral distribution of variable carbon stars J/A+A/321/236 J/A+A/321/236 Reddening and fluxes of carbon stars Interstellar extinction and the intrinsic spectral distribution of variable carbon stars A Knapik J Bergeat Astron. Astrophys. 321 236 1997 1997A&A...321..236K III/156 : General Catalog of Cool Galactic Carbon Stars, (Stephenson 1989) II/139 : General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988) II/140 : New Catalogue of Suspected Variable Stars (Kukarkin+, 1982) II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) Reddening Stars, carbon Stars, variable dust, extinction stars: AGB and post-AGB stars: carbon This table contains our CV-classification (see Subsec. 3.3 in the paper) for 133 carbon variables and their colour excess E(B-V) as determined by the method described in Sec. 4.
CV-classification and colour excess of 133 carbon variables. GCCS Stephenson's (1989) Cat. <III/156> Catalogue entry --- name GCVS or NSV or IRAS entry number=1 GCVS, General Catalogue of Variable Stars, Cat. <II/139> NSV, New Suspected Variables, Cat. <II/140> IRAS, IRAS Point Source Catalog, Cat. <II/125> --- GLON Galactic longitude deg GLAT Galactic latitude deg CV Carbon Variable classification (1 to 6) --- E(B-V) Excess in the B-V colour index mag table3.tex LaTeX version of table3 J. Bergeat CRAL-Observatoire de Lyon, Patricia Bauer CDS 1996 Oct 25 Jacques BERGEAT <jb@image.univ-lyon1.fr> J_A+A_321_236.xml SiO production in interstellar shocks. J/A+A/321/293 J/A+A/321/293 SiO production in interstellar shocks SiO production in interstellar shocks. P Schilke C M Walmsley G Pineau des Forets D R Flower Astron. Astrophys. 321 293 1997 1997A&A...321..293S Atomic physics Interstellar medium ISM: abundances ISM: jets and outflows ISM: molecules molecular processes shock waves We study the production of SiO in the gas phase of molecular outflows, through the sputtering of Si-bearing material in grains. The sputtering is driven by neutral particle impact on charged grains in C-type shocks, at the speed corresponding to ambipolar diffusion. Shock speeds in the range 10<v_s_<40km/s and preshock densities 10^4^<n_H_<10^7^cm^-3^ have been investigated. Sputtering of Si-bearing material in both the cores and the mantles of the grains is considered. We find that, for v_s_ of approximately 25km/s and n_H_ of the order 10^5^cm^-3^, column densities of SiO similar to those observed in molecular out flow regions can be generated by either mechanism. Impact by particles heavier than helium dominates the core-sputtering process for shock velocities of this order. The profiles of rotational transitions of SiO are computed and compared with observations of molecular outflows.
*Mantle and dissociative sputtering parameters Type a: mantle sputtering, b: dissociative sputtering --- R1 Beginning species of the reaction number=1 Asterisks denote species in grain mantles --- R2 Resulting species of the reaction --- S Sputtering yield factor --- Eth Sputtering threshold energy eV *Dissociation on impact parameters Type c: dissociation on impact --- R1 Beginning species of the reaction --- R2 Resulting species of the reaction --- Y0 Multiplicative constant number=1 The dissociative probability has an Arrhenius form, Y0exp(-Ediss/E), where E is the impact energy, Ediss the dissociation energy and Y0 the multiplicative constant --- Ediss Dissociation energy number=1 The dissociative probability has an Arrhenius form, Y0exp(-Ediss/E), where E is the impact energy, Ediss the dissociation energy and Y0 the multiplicative constant --- Rate coefficient parameters, for gas-phase reactions involving Si-bearing species R1 Beginning species of the reaction --- R2 Resulting species of the reaction --- gamma Gamma coefficient number=1 Rate coefficient : gamma.(T/300)^alpha^.exp(-beta/T) cm^3^/s --- alpha Alpha coefficient number=1 Rate coefficient : gamma.(T/300)^alpha^.exp(-beta/T) cm^3^/s --- beta Beta coefficient number=1 Rate coefficient : gamma.(T/300)^alpha^.exp(-beta/T) cm^3^/s K Note Note number=2 1: Langer & Glassgold, 1990, ApJ 352, 123 2: Supposed to be the same as CH (Gredel, 1990) 3: MacKay, 1995MNRAS.274..694M 4: UMIST ratefile (Millar et al., 1996, A&AS, in press) 5: Herbst (1995, private communication) 6: Elkin & Armentrout, 1984, J. Phys. Chem. 88, 5454 7: See the discussion of Flower et al., 1996MNRAS.280..447F --- Patricia Bauer CDS 1996 Sep 30 J_A+A_321_293.xml Effects of star cluster evolution on emission line ratios and the application to H II galaxies. Including a calibration of the R_23_ vs. 12+log(O/H) relationship J/A+A/321/29 J/A+A/321/29 Star cluster evolution Effects of star cluster evolution on emission line ratios and the application to H II galaxies. Including a calibration of the R_23_ vs. 12+log(O/H) relationship K Olofsson Astron. Astrophys. 321 29 1997 1997A&A...321...29O Models, evolutionary galaxies: evolution galaxies: starburst galaxies: stellar content A model of spectral evolution of star forming galaxies of various metallicity has been used to study the relation between the optical emission line ratio R_23_=([OII]{lambda}3727+[OIII]{lambda}{lambda}4959,5007)/H{beta} and the nebular oxygen abundance. It is shown that the scatter in an empirical comparison sample could be due to various upper stellar mass limits or different slopes of the stellar initial mass function in these objects.
Data of figs. 10 and 11 (extended). logQ(H) Number of Lyman continuum photon --- No Running number --- 12+log(O/H) Oxygen abundance --- R23 R23 ([OII]3727+[OIII]4959,5007)/Hbeta) value --- R33 R33 ([OIII]4363+[OIII]4959,5007)) value --- T Temperature of ionizing radiation K fig1.ps Empirical logR_23_ oxygen abundance relation. fig2.ps Evolutionary effects on the [OIII]5077/Hbeta emission line ratio. fig3.ps Evolution of the emission line ratio [OIII]3727/Hbeta. fig4.ps Effect of temporal evolution on the total number of Lyman continuum photons emitted from stellar populations of various metallicity fig5.ps R_23_ versus oxygen abundance relation. fig6.ps Effects of a non-instantaneous burst of star formation on the R_23_ versus oxygen abundance relation. fig7.ps R_23_ versus oxygen abundance under different assumptions about the slope of the IMF and the upper mass limit. fig8.ps Theoretical temporal evolution of R_23_ using an instantaneous burst of star formation. fig9.ps Effects of a non-instantaneous burst of star formation on the R_23_ versus oxygen abundance relation. fig10.ps R_23_ versus oxygen abundance calculated in the interval log(Q(H))=49.0-53.0. fig11.ps R_33_ versus oxygen abundance calculated in the interval log(Q(H))=49.0-53.0. fig12.ps Objects of Masegosa et al. (1994) as well as Davidson and Kinman (1985) plotted in intervals of T_ion_ in the R_23_ versus oxygen abundance plane. fig13.ps Calibrated R_23_ versus oxygen abundance relation. Patricia Bauer CDS 1996 Aug 12 J_A+A_321_29.xml Nebular gas abundances and mixing processes in the ringed galaxy NGC 4736 J/A+A/321/363 J/A+A/321/363 NGC 4736 H II regions properties Nebular gas abundances and mixing processes in the ringed galaxy NGC 4736 P Martin J Belley Astron. Astrophys. 321 363 1997 1997A&A...321..363M Galaxies, ring H II regions galaxies: abundances galaxies: evolution galaxies: individual (NGC 4736) galaxies: ISM galaxies: kinematics and dynamics galaxies: spiral Results of imaging spectrophotometry in the nebular lines H{alpha}, H{beta}, [O III]{lambda}5007 and [N II]{lambda}6584 of 65 H II regions in the early-type ringed galaxy NGC 4736 are presented. The oxygen abundance is derived using the line ratios [O III]/H{beta} and [N II]/[O III] as calibrated by Edmunds & Pagel (1984MNRAS.211..507E). Analysis of the O/H distribution in the bright resonance ring of star formation in NGC 4736 reveals that the O/H scatter is similar to that of the ISM of the disc of gas-rich galaxies, despite the very high star formation rate presently observed in the ring. The magnitude of azimuthal mixing induced by supernovae explosions and galaxy differential rotation is estimated in the ring; it is found that both can explain the small O/H dispersion observed in this structure. The radial distribution of O/H in the disc of NGC 4736 is also studied. Although the number of H II regions located outside the ring, and for which a reliable O/H value was obtained is limited, a slope for the global gradient is derived and found to be moderate (~-0.035+/-0.020dex/kpc). This gradient is shallower than gradients observed in normal galaxies, and is comparable to the slopes found for galaxies with bars of medium strength. Two evolutionary scenarios are proposed to explain this O/H distribution: i) Oval distortions, like bars, induce large-scale gas flows throughout the disc of NGC 4736, resulting in radial mixing of the chemical composition on a relatively short time scale (<=1Gyr); ii) A strong bar was present in the recent past and has flattened the abundance gradient.
NGC 4736 12 50.9 +41 07
Sample of HII regions in NGC 4736 Region Region number --- Xpos X position number=1 X and Y positions relative to the galaxy center, north and east are positive arcsec Ypos Y position number=1 X and Y positions relative to the galaxy center, north and east are positive arcsec AP Code for the size of square apertures used to measure the integrated fluxes number=2 1: 4 arcsec^2^; 2: 12 arcsec^2^; 3: 24 arcsec^2^ --- Properties of HII regions in NGC 4736 Region Region number --- log([OIII]/Hbeta) De-reddened [OIII]/Hbeta line ratio number=1 [OIII]/Hbeta = 1.35I([OIII]lambda5007)/I(Hbeta) --- e_log([OIII]/Hbeta) rms uncertainty on log([OIII]/Hbeta) --- log([NII]/[OIII]) De-reddened [NII]/[OIII] line ratio number=2 [NII]/[OIII] = I([NII]lambda6584)/I([OIII]lambda5007) --- e_log([NII]/[OIII]) rms uncertainty on log([NII]/[OIII]) --- Dist Galactocentric distance corrected for galaxy inclination kpc log(c(Hbeta)) Logarithmic extinction at Hbeta ---- (O/H)EP 12 + log(O/H) derived from the [OIII]/Hbeta ratio calibrated by EP number=3 EP: Edmunds & Pagel (1984MNRAS.211..507E) --- (O/H)A 12 + log(O/H) derived from the ratio [NII]/[OIII] calibrated by EP (3) number=4 Ratio [NII]/[OIII] from Alloin et al. (1979A&A....78..200A) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Sep 03 J_A+A_321_363.xml Quantitative analysis of the FUV, UV and optical spectrum of the O3 star HD 93129A J/A+A/321/531 J/A+A/321/531 Quantitative analysis of HD 93129A Quantitative analysis of the FUV, UV and optical spectrum of the O3 star HD 93129A G Taresch R P Kudritzki M Hurwitz S Bowyer A W A Pauldrach J Puls K Butler D J Lennon S M Haser Astron. Astrophys. 321 531 1997 1997A&A...321..531T Spectra, ultraviolet ISM: abundances ISM: molecules stars: atmospheres stars: fundamental parameters stars: individual (HD 93129A) X-rays: stars The tables contain the line identification lists used in the analysis. The wavelength (in Angstrom), ion, transition, f-value and interstellar components are listed for both the FUV and optical regions.
HD 93129 A 10 43 57.4 -59 32 51
</tableLink> <tableLink xlink:href="t optical.dat"> <title/> </tableLink> </tableLinks> <fields> <field> <name>lambda</name> <definition>Wavelength</definition> <units>0.1nm</units> </field> <field> <name>Ion</name> <definition>Ion designation</definition> <units>---</units> </field> <field> <name>Trans</name> <definition>Transition</definition> <units>---</units> </field> <field> <name>f</name> <definition>f-value</definition> <units>---</units> </field> <field> <name>Interst</name> <definition>Interstellar components</definition> <units>---</units> </field> </fields> </tableHead> <textFile xlink:href="tables.tex"> <name>tables.tex</name> <description> <para>LaTeX version of the tables</para> </description> </textFile> <history> <ingest> <creator> <lastName>Patricia Bauer</lastName> <affiliation>CDS</affiliation> </creator> <date> <year>1997</year> <month>Jun</month> <day>13</day> </date> <acknowledgement>Keith Butler <butler@usmu01.usm.uni-muenchen.de></acknowledgement> </ingest> </history> <identifier>J_A+A_321_531.xml</identifier> </dataset> <dataset subject="astronomy" xmlns:xlink="http://www.w3.org/XML/XLink/0.9"> <title>The "human" statistics of terrestrial impact cratering rate J/A+A/321/L33 J/A+A/321/L33 Terrestrial impact cratering rate The "human" statistics of terrestrial impact cratering rate L Jetsu Astron. Astrophys. 321, L33 ??? ??? 1997 1997A&A...321L..33J Earth comets: general Earth methods: statistical solar neighborhood The most significant periodicities in the terrestrial impact crater record are due to the "human-signal": the bias of assigning integer values for the crater ages. This bias seems to have eluded the proponents and opponents of real periodicity in the occurrence of these events, as well as the theorists searching for an extraterrestrial explanation for such periodicity. The "human-signal" should be seriously considered by scientists in astronomy, geology and paleontology when searching for a connection between terrestrial major comet or asteroid impacts and mass extinctions of species.
Ages of the impact craters Seq Sequential number --- Name Crater name --- Country Country --- t Age of the impact crater Myr e_t rms uncertainty on age Myr et1/et2 (e_t1/e_t2) for combined events Myr Diam Diameter km D1/D2 (D1/D2) for combined events km Loc Location for combined events --- C1 Y: in the C1 sample --- C2 Y: in the C2 sample --- C3 Y: in the C3 sample --- C4 Y: in the C4 sample --- C5 Y: in the C5 sample --- C6 Y: in the C6 sample --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1997 May 23 Lauri J. Jetsu <jetsu@norsg1.nordita.dk> J_A+A_321_L33.xml The Barium stars in the Hertzsprung-Russell diagram J/A+A/321/L9 J/A+A/321/L9 Barium stars in the HR diagram The Barium stars in the Hertzsprung-Russell diagram J Bergeat A Knapik Astron. Astrophys. 321, L9 ??? ??? 1997 1997A&A...321L...9B Magnitudes, absolute Stars, barium Hertzsprung-Russell (HR diagram) stars: chemically peculiar stars: evolution Table2 is an extension of Table 1 to 15 additional stars with slightly less accurate parallaxes (see text). The entries are the same in both tables.
The data for 37 Ba stars The data for 15 Ba stars HD Henry Draper Catalogue (Cat. <III/135>) or Lu (1991, Cat. <V/81>) entry --- G Spectral group (see Sect. 2 of paper) --- E(B-V) Colour excess of interstellar extinction mag Mvl Lower estimate of Mv mag Mv Absolute visual magnitude number=1 Absolute visual magnitude between the lower and upper estimates as derived in Sect. 3 mag Mvu Upper estimate of Mv mag LumClass Proposed luminosity class number=2 Proposed luminosity class (Sect. 4). III = IIIab II- : possibly IIIa IIIa- : possibly III IIIb- : possibly IVa IVb- : possibly Va --- tables.tex LaTeX version of the tables J. Bergeat CRAL-Observatoire de Lyon 1997 Mar 28 Jacques Bergeat <jb@image.univ-lyon1.fr> J_A+A_321_L9.xml H_2_O maser emission from irregular variables J/A+A/322/159 J/A+A/322/159 H2O maser emission from irregular variables H_2_O maser emission from irregular variables M Szymczak D Engels Astron. Astrophys. 322 159 1997 1997A&A...322..159S Stars, masers Stars, variable circumstellar matter masers radio lines: stars stars: AGB and post-AGB stars: mass-loss We have performed a search for the 22 GHz water maser line among 72 optically identified irregular and semiregular red variables. New detections were made of five stars, while only four of nine objects previously known as maser sources were redetected. The probability for the detection of H_2_O maser emission increases with V light amplitude, and with H-K and K-[12] colours just as in regular Mira and semiregular variables of SRa- and SRb-types. The detection rate of water masers is about 25% for nearby Lb objects (D<400pc) in the sample, comparable to that observed in the SRa and SRb stars. No masers were detected in objects with mass loss rates <=4x10^-8^M_{sun}_/yr. Maser luminosities are 10^41^-10^43^photons/s similar to that of the bluest Miras and typical SRa and SRb stars showing water maser emission. A comparison of our data on irregular stars with those previously obtained on SRa and SRb variables suggests that most radio and infrared properties are indistinguishable among both classes of objects.
Upper limits for the undetected irregular and semiregular stars GCVS GCVS name --- ref references for H_2_O detection number=1 References: a: H_2_O maser (unpublished Effelsberg data) b: H_2_O maser (Dickinson 1976ApJS...30..259D) --- IRAS IRAS name --- Mtype Morphological type --- Date Observation date "M/YY" 3sigma 3 sigma upper limit Jy Patricia Bauer CDS 1997 May 27 Marian Szymczak <msz@.astro.uni.torun.pl> J_A+A_322_159.xml Critical tests of stellar evolution in open clusters. II. Membership, duplicity, and stellar and dynamical evolution in NGC 3680 J/A+A/322/460 J/A+A/322/460 NGC 3680 photometry and radial velocities Critical tests of stellar evolution in open clusters. II. Membership, duplicity, and stellar and dynamical evolution in NGC 3680 B Nordstrom J Andersen M I Andersen Astron. Astrophys. 322 460 1997 1997A&A...322..460N J/A+AS/118/407 : CCD photometry & velocities of NGC 3680 stars, Paper I (Nordstroem+ 1996) Clusters, open Photometry Radial velocities Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 3680) stars: evolution stars: fundamental parameters stars: kinematics stars: luminosity function, mass function Based on new, accurate photometry, radial velocities, and proper motions for the intermediate-age open cluster NGC 3680, we identify individual single and binary cluster members and field stars in the colour-magnitude diagram (CMD). This basic step turns out to be crucial for a proper understanding of the cluster CMD: ~60% of the stars are found to be field stars, and over 50% of the cluster stars are binaries. No bona fide cluster star is found more than 1.5mag below the turnoff, and cluster stars below 1.4M_{sun}_ are only found in binary systems. The total present mass of NGC 3680 is ~100M_{sun}_, excluding any as yet unseen stellar remnants, and its half-mass radius is 3.3' (1.2pc). Comparison with plausible IMFs indicates that only ~3% of the original stars and <~10% of the mass now survive, ~30% of the initial mass being in the form of massive stars that have now completed their evolution, and ~60% in low-mass stars which may now be located in a distant cluster halo or perhaps have been lost entirely. The single main-sequence cluster members form an extremely tight sequence in the CMD, with E_(b-y)_=0.034 and [Fe/H]=+0.11. A direct fit to the Hyades main sequence yields (m-M)_0_=10.5+/-0.2 for NGC 3680. Isochrones from several stellar models have been fit to the cluster sequence. When based on consistent uvby colour transformations and the above cluster parameters, these fits are very stable and show that standard models are not acceptable for stars with the turnoff mass of NGC 3680. Overshooting models perform much better, but further refinement of the overshooting formalism seems to be needed. The age derived for NGC 3680 is 1.45+/-0.3Gyr. The limiting factor in a precise comparison of theory and observations is now the transformation from theoretical to observed parameters, particularly (broad-band) colours.
NGC 3680 11 25.7 -43 15
Summary data for 120 stars in the field of NGC 3680 Id Identification number (see paper) --- Vmag V magnitude mag b-y b-y colour index mag n_b-y M for missing entry --- B-V B-V colour index mag n_B-V M for missing entry --- RV Mean radial velocity km/s n_RV M for missing entry --- e_RV Mean error of mean radial velocity km/s n_e_RV M for missing entry --- pRV Radial velocity membership probability (%) --- n_pRV M for missing entry --- pPM Proper motion membership probability (%) --- n_pPM M for missing entry --- Note1 Remarks on binary stars --- Note2 Remarks on final membership assignment --- Patricia Bauer CDS 1997 Jun 09 Birgitta Nordstrom <birgitta@bro730.astro.ku.dk> J_A+A_322_460.xml Properties of theoretical RRab light curves J/A+A/322/817 J/A+A/322/817 Theoretical RRab light curves properties Properties of theoretical RRab light curves M U Feuchtinger E A Dorfi Astron. Astrophys. 322 817 1997 1997A&A...322..817F Stars, variable methods: numerical stars: interiors stars: oscillations stars: variables: other Using an adaptive radiation hydrodynamics code we have computed a grid of fundamental mode RR Lyrae models in order to give a detailed comparison to observed RR Lyrae light curves and to investigate the influence of several numerical parameters inherent to the computational method. The results can be summarized as follows: Concerning the comparison to observations the proposed solution of the well known RR Lyrae phase discrepancy in Feuchtinger & Dorfi (1996A&A...306..837F) is corroborated on the basis of more than 50 models. It is shown how the Fourier parameters vary during the crossings of the instability strip. Based on the large number of theoretical models we can study the properties of theoretical RRab light curves and e.g. state that no clear relation exists which links the fundamental stellar parameters to the low order Fourier coefficients. Investigating the long term evolution and the influence of several critical parameters like numerical viscosity, number of grid points or switching temperature between Lagrangian and adaptive grid, it turns out that the Fourier parameters are essentially independent on the special choice of our numerical parameters.
Stellar parameters of the models and parameters of the resulting nonlinear light curves Mass Mass solMass L Luminosity solLum Teff Effective temperature K Z Metallicity --- dL Bolometric luminosity amplitude mag P0 Fundamental period d R21 Fourier amplitude (A2/A1 ratio) --- Phi21 Fourier phase (P2 - 2P1 value) --- Phi31 Fourier phase (P3 - 3P1 value) --- A0 Fundamental Fourier amplitude --- A1 First harmonic Fourier amplitude --- A2 Second harmonic Fourier amplitude --- A3 Third harmonic Fourier amplitude --- P1 First harmonic Fourier phase --- P2 Second harmonic Fourier phase --- P3 Third harmonic Fourier phase --- Patricia Bauer CDS 1997 Jan 07 Michael U. Feuchtinger <FM@amok.ast.univie.ac.at> J_A+A_322_817.xml The symbiotic star YY Her. I. Photometric history over 1890-1996. J/A+A/323/113 J/A+A/323/113 YY Her photometric history over 1890-1996 The symbiotic star YY Her. I. Photometric history over 1890-1996. U Munari M Rejkuba M Hazen J Mattei E Schweitzer R Luthardt S Shugarov B F Yudin A A Popova P V Chugainov G Sostero A Lepardo Astron. Astrophys. 323 113 1997 1997A&A...323..113M Photometry Stars, variable binaries: symbiotic stars: individual (YY Her) Table 5 presents AAVSO and AFOEV amateur astronomer's data combined into 30-day bins. <JD> is the mean JD of the bin, <m-vis> is the mean of N visual estimates after correction for systematic offsets (two decimal figures only for N>=2); sigma(<m-vis>) is the error of the mean. Table 6 lists photographic m(pg) magnitudes of YY Her. The various sources of data and instruments are given for each magnitude. The upper limits are flagged by >, while the uncertain values have the : or :: flag.
YY Her AS 297 MH-alpha 352-34 18 14 34 +20 59 12
visual photometry bin Progressive bin number --- <JD> Julian date d <m-vis> Mean visual magnitude mag n_<m-vis> Number of visual estimates in the bin --- e_<m-vis> Error of the mean visual magnitude mag photographic m(pg) photometry Source Source of the data Harvard = Harvard plate archive Crimea = Crimea plate archive Carte d.C. = Carte du Ciel atlas POSS = Palomar atlas Sonneberg = Sonneberg plate archive --- Instr. Instrument H1 = 20 cm Draper refractor H2 = 20 cm refractor H3 = 40 cm Metcalf refractor H4 = 25 cm Metcalf refractor H5 = recent patrol series H6 = recent 4 cm patrol series H7 = very wide angle 4 cm patrol series PS = Palomar Schmidt telescope CC = Carte du Ciel (Paris zone) C1 = 9.6/64 cm refractor C2 = 16/82 cm refractor C3 = 40/160 cm refractor S1 = Tessar camera, 1:4.5, f= 250 mm --- JD Julian date d l_mpg Limit flag on mpg --- mpg Photographic m(pg) magnitude mag u_mpg Uncertain flag on mpg --- Patricia Bauer CDS 1997 Feb 26 Marina Rejkuba <rejkuba@astras.pd.astro.it> J_A+A_323_113.xml Pleiades low-mass binaries: do companions affect the evolution of protoplanetary disks? J/A+A/323/139 J/A+A/323/139 K magnitude of Pleiades low-mass binaries Pleiades low-mass binaries: do companions affect the evolution of protoplanetary disks? J Bouvier F Rigaut D Nadeau Astron. Astrophys. 323 139 1997 1997A&A...323..139B I/163 : US Naval Observatory Pleiades Catalog (Van Flandern 1969) Photometry Stars, double and multiple Stars, pre-main sequence binaries: close circumstellar matter open clusters and associations: individual (Pleiades, Melotte 22) stars: formation stars: pre-main sequence stars: rotation This table provides the list of stars observed but not resolved during the diffraction-limited survey of G and K Pleiades dwarfs. Previously known binaries, either photometric or spectroscopic, are referenced.
Pleiades Melotte 22 03 47.0 +24 07
Unresolved Pleiades dwarfs Name Object name --- Kmag K magnitude (rms = 0.05 mag) mag Bin Binarity: PB = photometric binary, SB = spectroscopic binary --- Ref References number=1 1 = Stauffer (1984ApJ...280..189S) 2 = Mermilliod et al. (1992A&A...265..513M) 3 = Stauffer & Hartmann (1987ApJ...318..337S) --- Patricia Bauer CDS 1997 Jan 07 Jerome Bouvier <bouvier@cfht.hawaii.edu> J_A+A_323_139.xml The morphological segregation of galaxies in clusters. III. The distant cluster Cl 0939+4713 (Abell 851) J/A+A/323/337 J/A+A/323/337 Abell 851 morphological segregation The morphological segregation of galaxies in clusters. III. The distant cluster Cl 0939+4713 (Abell 851) S Andreon E Davoust T Heim Astron. Astrophys. 323 337 1997 1997A&A...323..337A J/A+AS/116/429 : Classification of Coma early galaxies (Andreon+ 1996) Clusters, galaxy Galaxies, photometry galaxies: evolution galaxies: fundamental parameters galaxies: individual (Coma cluster, 0939+4713, Abell 851) galaxies: luminosity function, mass function We have performed an isophotal analysis of galaxies in the distant (z=0.4) cluster Cl0939+4713 (Abell 851), using post-refurbished Hubble Space Telescope images. Morphological type estimates for the galaxies are given. A rigorous comparison of the properties of the types shows that early-type galaxies in Cl0939+4713 are, within the present statistical or systematic errors, indistinguishable from their counterparts in Coma in all their studied properties, namely ellipticity profile, slope of the color-magnitude relation from the near-ultraviolet to the near-infrared colors, mean surface brightness and luminosity function in the restframe photographic J band, homogeneity in color (around the color-magnitude relation). Furthermore ellipticals and lenticulars are separately homogeneous in their mean surface brightness, and have similar relative mean surface brightnesses in both clusters. Spirals are overabundant in Cl0939+4713 with respect to Coma, but twice less than previously estimated, and are more similar to field spirals than to cluster spirals. We suggest that the differences in the photometric properties of the spirals in the two clusters arise from differences in cluster gas density distribution which ultimately bring star formation in the spirals to a stop in Coma, but not in Cl0939+4713. The morphological types are segregated along a privileged direction that coincides with the position angle of the major axis of the outer X-ray isophotes in the cluster, just like in Coma and Perseus.
ACO 851 Cl 0939+4713 09 42.8 +47 00
*Photometric parameters and classification of the galaxies in the sample No No in the Dressler & Gunn (1992) catalogue Cat. <J/ApJS/78/1> --- log(Rad) logarithm of the approximate effective radius arcsec Dphot Photometric evidence for a disk number=1 st strong, cl clear, ft faint, no none --- b/a Typical axis ratio, either its minimum value, if clearly defined, or its value at the effective isophote in other cases --- Loc(b/a) Location where the typical axis ratio was estimated number=2 ex for the extremum, re for the effective isophote, co if the value is the same at both locations --- e4 Typical e4 parameter, either its extremum value, if clearly defined, or its value at the effective isophote in other cases. % Loc(ce4) Location where e_4 was estimated number=2 ex for the extremum, re for the effective isophote, co if the value is the same at both locations --- b/aE Axis ratio in the envelope, i.e. at the isophote F702W~25mag/arcsec+2 --- Amp Amplitude of isophotal twist in the range of reliable measurements. deg n_Amp Note on amplitude number=3 ':' : uncertainty flag n : when the twist is difficult to be measured, as the isophotes are nearly circular --- Bar Detection of a bar number=4 bar: bar seen bar?: bar suspected no: no bar seen --- Disk Detection and classification of a disk number=5 emDi: embedded disk miDi: mixed disk exDi: extended disk ?Di: detected but unclassified disk no: no disk seen --- Spiral Detection of a spiral pattern number=6 spiP: spiral pattern seen spiP?: spiral pattern suspected no: no spiral pattern seen --- Envelop Classification of an envelope number=7 spH: spheroidal halo thD: thick disk exD: extended disk pec: peculiar envelope ? : unclassified envelope --- MType morphological classification number=8 boE: boxy E unE: undetermined E diE: disky E SA0, SAB0, SB0, Sa, ...: as usual S: spiral of unknown stage SB..: barred spiral of unknown stage unre: unresolved --- Note An asterisk refers to notes about specific features such as important dust pattern, ring or lens, low SuBr, f4-asymmetry, etc. and about uncertainties of various sources number=9 Individual notes: 137: roundish galaxy, pear-shaped at intermediate radii, large twist in the envelope. SA0 galaxy with dust unresolved? 138: very irregular isophotes. 150: asymmetric in the outer regions. 190: irregular isophotes. 191: warp. 211: probably barred. 215: possible error of Dressler et al. (1994) in HST WF-PC1 identification. 225: irregular isophotes, HII regions. 269: uncertain type, because near the edge of the image. 292: more concentrated than DG 385. 293: arms and HII regions. 294: HII regions. 299: outer irregular isophotes. 302: difficult case, r^1/4^ SuBr profile, boxy if anything. 310: various clumps superposed. 311: interacting, dust, ring. 312: arms and HII regions. 316: arms and HII regions. 318: within the halo of DG 311 - tidal extension. 320: arms, HII regions and dust. 329: HII regions, dust. 339: pear-shaped isophotes (e3,f3{dif}0) at the r_e. 348: arms - beautiful spiral, HII regions. 360: edge-on, warped. 363: tail at low subr, difficult classification due to the smallness of the galaxy. 365: pear-shaped at low SuBr, nearby straight object (arclet?) and a galaxy at 1". 366: boxy bulge, f4 asymmetry. 367: boxy inside 1 arcsec. 371: arm, HII regions. 375: strange companion galaxy(?). 377: larger component of pair probably unresolved from WF1. 383: arms. 384: S? irregular isophotes - dust? 385: r^1/4^ profile, unresolved. 393: near the edge of the image. 397: superposed stars probably explain WF1 classification. 400: roundish galaxy. 408: slight evidence for a disk. 409: elongated galaxy with flat profile. 413: roundish galaxy with r^1/4^ profile, irregular outer isophotes, and constant positive e4. 422: non-concentric isophotes, tidal extension, possibly interacting with DG 439. 431: the companion galaxy DG 436 shows disturbances. 432: r^1/4^ profile but asym. isophotes similar to the GMP 1646 irregular galaxy in Coma, difficult classification. 434: irregular asymmetric. 436: possibly interacting with DG 431, tidal extension, irregular isophotes, halo offcentered. 439: arms and dust. 441: edge-on, type uncertain because small asymmetry points toward S. 448: faint galaxy. 451: HII regions, possibly interacting with DG 458 because common envelope. 454: asymmetric. 457: face-on, two-component galaxy (bulge+disk). 458: roundish object, possibly interacting with DG 451. 462: irregular isophotes. 471: dust. --- table1.tex TeX version of table1 Patricia Bauer CDS 1996 Dec 03 Andreon Stefano <andreon@cerere.na.astro.it> J_A+A_323_337.xml Circumstellar C_2_, CN, and CH^+^ in the optical spectra of post-AGB stars J/A+A/323/469 J/A+A/323/469 Optical spectra of post-AGB stars Circumstellar C_2_, CN, and CH^+^ in the optical spectra of post-AGB stars E J Bakker E F van Dishoeck L B F M Waters T Schoenmaker Astron. Astrophys. 323 469 1997 1997A&A...323..469B Line Profiles Spectroscopy circumstellar matter line: identification molecular processes stars: AGB and post-AGB We present optical high-resolution spectra of a sample of sixteen post-AGB stars and IRC +10216. Of the post-AGB stars, ten show C_2_ Phillips (A^1^{PI}_u_-X^1^{SIGMA}^+^_g_) and Swan (d^3^{PI}_g_-a^3^{PI}_u_) and CN Red System (A^2^{PI}-X^2^{SIGMA}^+^) absorption, one CH^+^ (A^1^{PI}-X^1^{SIGMA}^+^) emission, one CH^+^ absorption, and four without any molecules. We find typically T_rot_ ~43-399, 155-202, and 18-50K, logN~14.90-15.57, 14.35, and 15.03-16.47cm^-2^ for C_2_, CH^+^, and CN respectively, and 0.6<=N(CN)/N(C_2_)<=11.2. We did not detect isotopic lines, which places a lower limit on the isotope ratio of ^12^C/^13^C>20. The presence of C_2_ and CN absorption is correlated with cold dust (T_dust_<=300K) and the presence of CH^+^ with hot dust (T_dust_>=300K). All objects with the unidentified 21{mu}m emission feature exhibit C_2_ and CN absorption, but not all objects with C_2_ and CN detections exhibit a 21{mu}m feature. The derived expansion velocity, ranging from 5 to 44km/s, is the same as that derived from CO millimeter line emission. This unambiguously proves that these lines are of circumstellar origin and are formed in the AGB ejecta (circumstellar shell expelled during the preceding AGB phase). Furthermore there seems to be a relation between the C_2_ molecular column density and the expansion velocity, which is attributed to the fact that a higher carbon abundance of the dust leads to a more efficient acceleration of the AGB wind. Using simple assumptions for the location of the molecular lines and molecular abundances, mass-loss rates have been derived from the molecular absorption lines and are comparable to those obtained from CO emission lines and the infrared excess.
IRAS 04296+3429 04 32 56.6 +34 36 11 IRAS 05113+1347 05 14 07.9 +13 50 28 IRAS 05341+0852 05 36 54.2 +08 54 10 HD 44179 06 19 58.2 -10 38 14 HD 56126 IRAS 07134+1005 07 16 10.2 +09 59 48 IRAS 08005-2356 08 02 40.5 -24 04 43 IRC +10216 IRAS 09452+1330 09 47 57.2 +13 16 44 IRAS 20000+3239 20 01 59.4 +32 47 32 AFGL 2688 21 02 18.7 +36 41 38 IRAS 22223+4327 22 24 30.6 +43 43 03 HD 235858 IRAS 22272+5435 22 29 10.3 +54 51 06 IRAS 23304+6147 23 32 44.9 +62 03 49 HD 213985 IRAS 22327-1731 22 35 27.4 -17 15 27
Physical parameters derived from molecular lines Reaction Reaction considered number=1 1: C_2_ A^1^PI_u_ - X^1^SIGMA^+^_g_ (3,0) or (2,0) (C2 (2,0) for IRC +10216, else C2 (3,0)) and CN A^2^PI - X^2^SIGMA^+^ (2,0) or (3,0) (CN (2,0) for IRAS 08005-2356, HD 235858, and IRC +10216, else CN (3,0)) 2: CH^+^ A^1^PI - X^1^SIGMA^+^ (0,0) --- Name Object name --- n_Name Note on name number=2 the emission line spectrum has been analyzed with A^1^{PI} J'=0 as energy zero level. v_exp_ and T_rot_ are real, but the column density of HD 44179 is rather meaningless --- Vel C2 or CH+ velocity km/s e_Vel rms uncertainty on Vel km/s Vexp1 C2 or CH+ Vexp (+/-2.0) number=3 v_exp_=v_sys_-v_(Element) (Element = C_2_, CN or CH^+^) km/s Trot1 C2 or CH+ rotational temperature K e_Trot1 rms uncertainty on Trot1 K logNmol1 C2 or CH+ column density (+/-0.10) cm-2 logNmolSum C2 or CH+ column density sum over J'' or N'' levels of observed transitions cm-2 log(dM/dt)1 C2 Mass loss rate solMass/yr V(CN) CN velocity km/s e_V(CN) rms uncertainty on V(CN) km/s Vexp2 CN Vexp (+/-2.0) number=3 v_exp_=v_sys_-v_(Element) (Element = C_2_, CN or CH^+^) km/s Trot2 CN rotational temperature K e_Trot2 rms uncertainty on Trot2 K logNmol2 CN column density (+/-0.10) cm-2 log(dM/dt)2 CN Mass loss rate solMass/yr Dv v(CN) - V(C2) number=4 {delta}v= v_CN_-v_C_2__ km/s e_Dv rms uncertainty on Dv km/s N(CN)/N(C2) CN/C2 abundance ratio --- 12C/13C Upper limit (=>) for ^12^C/^13^C ratio --- C_2_ A^1^PI_u_-X^1^SIGMA^+^_g_ Phillips (2,0) band B Branch identification code number=1 Branch identification: -1: P branch ({DELTA}(J)=-1=J'-J") 0: Q branch ({DELTA}(J)=0=J'-J") 1: R branch ({DELTA}(J)=1=J'-J") --- J" Rotational quantum number, total angular momentum including spin (Herzberg 1950) --- Lambda Laboratory wavelength of transition in air 0.1nm f(J'J") Oscillator strength --- EW Equivalent width 0.1pm C_2_ A^1^PI_u_-X^1^SIGMA^+^_g_ Phillips (3,0) band B Branch identification code number=1 Branch identification: -1: P branch ({DELTA}(J)=-1=J'-J") 0: Q branch ({DELTA}(J)=0=J'-J") 1: R branch ({DELTA}(J)=1=J'-J") --- J" Rotational quantum number, total angular momentum including spin (Herzberg 1950) --- Lambda Laboratory wavelength of transition in air 0.1nm f(J'J") Oscillator strength --- EW(042) Equivalent width of IRAS 04296+3429 0.1pm EW(051) Equivalent width of IRAS 05113+1347 0.1pm EW(053) Equivalent width of IRAS 05341+0852 0.1pm EW(561) Equivalent width of HD 56126 0.1pm EW(080) Equivalent width of IRAS 08005-2356 0.1pm EW(102) Equivalent width of IRC +10216 0.1pm EW(200) Equivalent width of IRAS 20000+3239 0.1pm EW(268) Equivalent width of AFGL 2688 0.1pm EW(222) Equivalent width of IRAS 22223+4327 0.1pm EW(235) Equivalent width of HD 235858 0.1pm EW(233) Equivalent width of IRAS 23304+6147 0.1pm CN A^2^PI-X^2^SIGMA^+^ Red System (2,0) band B Branch identification code number=1 Branch identification: 1: R1, 2: Q1, 3: P1, 4: ^Q^R12, 5: ^P^Q12, 6: ^O^P12 7: R2. 8: Q2' 9: P2. 10: ^S^R21, 11: ^R^Q21, 12: ^Q^P21 --- J" Rotational quantum number, total angular momentum including spin (Herzberg 1950) --- N" Rotational quantum number, total angular momentum excluding spin (Herzberg 1950) number=2 For CN: J"=N"-1/2(F2), J"=N"+1/2(F2) --- Lambda Laboratory wavelength of transition in air 0.1nm f(J'J") Oscillator strength --- EW(080) Equivalent width of IRAS 08005-2356 0.1pm EW(102) Equivalent width of IRC +10216 0.1pm EW(235) Equivalent width of HD 235858 0.1pm CN A^2^PI-X^2^SIGMA^+^ Red System (3,0) band B Branch identification code number=1 Branch identification: 1: R1, 2: Q1, 3: P1, 4: ^Q^R12, 5: ^P^Q12, 6: ^O^P12 7: R2. 8: Q2' 9: P2. 10: ^S^R21, 11: ^R^Q21, 12: ^Q^P21 --- J" Rotational quantum number, total angular momentum including spin (Herzberg 1950) --- N" Rotational quantum number, total angular momentum excluding spin (Herzberg 1950) number=2 For CN: J"=N"-1/2(F2), J"=N"+1/2(F2) --- Lambda Laboratory wavelength of transition in air 0.1nm f(J'J") Oscillator strength --- EW(042) Equivalent width of IRAS 04296+3429 0.1pm EW(051) Equivalent width of IRAS 05113+1347 0.1pm EW(053) Equivalent width of IRAS 05341+0852 0.1pm EW(561) Equivalent width of HD 56126 0.1pm EW(200) Equivalent width of IRAS 20000+3239 0.1pm EW(268) Equivalent width of AFGL 2688 0.1pm EW(222) Equivalent width of IRAS 22223+4327 0.1pm EW(233) Equivalent width of IRAS 23304+6147 0.1pm CH^+^ A^1^PI-X^1^SIGMA^+^ (0,0) band B Branch identification code number=1 Branch identification: -1: P branch ({DELTA}(J)=-1=J'-J") 0: Q branch ({DELTA}(J)=0=J'-J") 1: R branch ({DELTA}(J)=1=J'-J") --- J" Rotational quantum number, total angular momentum including spin (Herzberg 1950) --- Lambda Laboratory wavelength of transition in air 0.1nm f(J'J") Oscillator strength number=2 f(J',J")=f_abs_ is the absorption oscillator strength, for emission g_J'_ f_em_ = g_J"_ f_abs_ --- EW(441) Equivalent width of HD 44179 0.1pm EW(213) Equivalent width of HD 213985 0.1pm tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Oct 09 Eric J. Bakker <ebakker@viking.as.utexas.edu> J_A+A_323_469.xml The nature of the FHIL winds from AGN J/A+A/323/707 J/A+A/323/707 Nature of the FHIL winds from AGN The nature of the FHIL winds from AGN U Erkens I Appenzeller S Wagner Astron. Astrophys. 323 707 1997 1997A&A...323..707E Active gal. nuclei Galaxies, spectra Line Profiles galaxies: active galaxies: nuclei galaxies: Seyfert line: profiles X-rays: galaxies In order to investigate the properties of the forbidden high-ionization lines (FHILs) in the spectra of AGN we observed 15 Seyfert galaxies and two emission line radio galaxies with a spectral resolution of about 2000 in the spectral range 3200-11000{AA}. All observed spectra contained significant [Ne V] and [Fe VII] lines. The spectra of the Seyfert nuclei (but not the radio galaxies) showed also [Fe X], [Fe XI], and in some cases [Fe XIV] emission. Our data confirm that the FHILs are on average broader and blueshifted relative to the lines of lower ionization stages. The amount of the blueshift was found to be correlated with the line widths. Large blueshifts were observed only for lines with high FWHM. An analysis of the line ratios indicates for the FHIL producing plasma an average electron temperature of about 7x10^4^K. Comparing our results with ROSAT data we found a correlation between the X-ray spectral index and the strength of the FHILs. Strong FHIL emission was found to occur predominantly in objects with a soft X-ray excess. We propose that the FHIL emission and the X-ray absorption edges in AGN ("warm absorbers") are related and that both phenomena result from a radiation driven warm wind originating in the central region of the AGN.
Reddening corrected line flux, velocity shift, and line widths measured in the spectrum AGN AGN name --- Ion Ion species --- lambda rest wavelength 0.1nm Flux Flux (in units Flux(H{beta})=1) --- e_Flux Mean error on Flux --- deltaV velocity shift km/s e_deltaV Mean error on velocity shift km/s FWHM FWHM km/s e_FWHM Mean error on FWHM km/s Observed H{beta} line flux AGN AGN name --- Flux(Hb) Normalised H{beta} flux 10-16W/m2 tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Jun 26 Monika Darr <M.Darr@lsw.uni-heidelberg.de> J_A+A_323_707.xml Line spectra of Liners. The contribution of the different ionization mechanisms. J/A+A/323/71 J/A+A/323/71 Line spectra of Liners Line spectra of Liners. The contribution of the different ionization mechanisms. M Contini Astron. Astrophys. 323 71 1997 1997A&A...323...71C Galaxies, spectra galaxies: active galaxies: Seyfert galaxies: starburst radiation mechanisms: non-thermal shock waves The physical conditions which characterize individual Liners are obtained by fitting the observational spectra of the Ho et al. (1993ApJ...417...63H) sample by model calculations. Composite models which consistently account both for shocks, accompanying the radial outward motion of the gaseous clouds, and a photoionizing radiation flux are used. Power-law or black body radiation is considered, depending on the characteristics of the line spectra. The SUMA code is used. The contributions of the different ionization mechanisms to the spectrum emitted by each object are calculated and compared with the observations. The most significant line ratios of Liner spectra are analyzed to show the relative importance of photoionization by radiation from the active center or from starbursts, of photoionization by diffuse radiation, and of collisional ionization by shocks. Model results show that [Ne V] lines can be strong due to collisional ionization and/or photoionization. Lines from the II and III ionization levels are usually due to photoionization, but a strong contribution by collisional ionization appears in case of high densities and/or of a strong shock. Neutral lines are enhanced by diffuse radiation. The contribution of high density gas to the line intensities in Liner spectra is very small, indicating that the high density region, located between the NLR and the BLR, is also small. The results show that shocks play an important role, even if a photoionizing flux is present. On average, higher than cosmic N/H and lower S/H are indicated. The physical characteristics of Seyfert galaxies and of starburst galaxies are confirmed. The satisfactory results obtained interpreting the heterogeneous observational sample by SUMA strengthen the hypothesis that shock signature in AGN spectra is due to cloud motions in galaxies.
Line intensities relative to Hbeta Model Model number=1 M0: Shock dominated model (F=0) M1: Model with low shock velocity (Vs), preshock density (n0) and photoionization flux (F) M2: Model with low Vs and n0, but relatively higher F M3: Model with low Vs and n0, but relatively higher F M4: Model showing the effect of a low high-energy cut-off M5: Model characterized by higher Vs and n0 which are higher limits deduced by observations of Liners spectra M1d: Model characteristic of higher density M3d: Model characteristic of higher density M6: represent starburst model M7: represent starburst model --- [NeV] Line intensity of [Ne V] 3426 (Hbeta=1) --- [OII] Line intensity of [O II] 3727+ (Hbeta=1) --- [NeIII] Line intensity of [Ne III] 3869+ (Hbeta=1) --- [OIII] Line intensity of [O III] 4363 (Hbeta=1) --- HeII Line intensity of He II 4686 (Hbeta=1) --- [OIII]b Line intensity of [O III] 5007+ (Hbeta=1) --- [NI] Line intensity of [N I] 5200+ (Hbeta=1) --- HeI Line intensity of He I 5876 (Hbeta=1) --- [OI] Line intensity of [O I] 6300+ (Hbeta=1) --- [NII] Line intensity of [N II] 6583+ (Hbeta=1) --- [SII] Line intensity of [S II] 6717 (Hbeta=1) --- [SII]b Line intensity of [S II] 6730 (Hbeta=1) --- [OII]b Line intensity of [O II] 7322+ (Hbeta=1) --- [SIII] Line intensity of [S III] 9402+ (Hbeta=1) --- Hbeta Hbeta flux mW/m2 R[OIII] Line ratio [O III]5007+/[O III]4363 --- R[OII] Line ratio [O II]3727+/[O II]7322 --- R[SII] Line ratio [S II]6717/[S II]6730 --- RN Line ratio [NII]/[N I] line ratio --- RHe Line ratio [He II]/[He I] line ratio --- Vs Shock velocity km/s n0 Preshock density cm-3 U Ionization parameter --- F Photoionizing power law radiation flux ph/cm+2/s/eV Ec High energy cutoff of radiation flux eV T Stellar temperature K Comparison of calculated spectra with observations (table2, part. 1) Ion Ion --- Line Line --- NGC Galaxy name --- Obs Observed line intensity --- Obs2 Observed line intensity from Ho et al. (1996ApJ...462..183H), NGC 3031 only. --- Calc Calculated line intensity --- Calc2 Calulated line intensity --- Calc3 Calculated line intensity --- Comparison of calculated spectra with observations (table2, part. 2) NGC Galaxy name --- HbObs Observed Hbeta flux mW/m2 HbCal Calculated Hbeta flux mW/m2 Vs Shock velocity km/s n0 Preshock density cm-3 T Stellar temperature K U Ionization parameter --- F Photoionizing power law radiation flux ph/cm+2/s/eV B0 Preshock magnetic field 10-4T N/H N/H line ratio --- O/H O/H line ratio --- Ne/H Ne/H line ratio --- S/H S/H line ratio --- Summary of the results presented in table2 No Number referring to diagnostic diagram --- NGC NGC number --- Type Classification number=1 H: H II region L: Liner S: Seyfert --- Vs Shock velocity km/s n0 Photoionizing power law radiation flux cm-3 F Photoionizing power law radiation flux ph/cm+2/s/eV U Ionization parameter --- T Star temperature K N/H Relative N/H ratio to cosmic one number=2 c: cosmic <: lower than cosmic >: higher than cosmic >=: higher or equal to cosmic value --- Ne/H Relative Ne/H ratio to cosmic one number=2 c: cosmic <: lower than cosmic >: higher than cosmic >=: higher or equal to cosmic value --- S/H Relative S/H ratio to cosmic one number=2 c: cosmic <: lower than cosmic >: higher than cosmic >=: higher or equal to cosmic value --- Flux Type of ionizing radiation responsible for heating and ionization of the emitting gas number=3 bb: black body os: only shock pl: power law --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Dec 03 Marcella Contini <contini@post.tau.ac.il> J_A+A_323_71.xml Radio-loud active galaxies in the northern ROSAT All-Sky Survey. II. Multi-frequency properties of unidentified sources J/A+A/323/739 J/A+A/323/739 ROSAT detected quasars. II. Radio-loud active galaxies in the northern ROSAT All-Sky Survey. II. Multi-frequency properties of unidentified sources W Brinkmann J Sieber E D Feigelson R I Kollgaard S A Laurent-Muehleisen W Reich E Fuerst P Reich W Voges J Truemper R McMahon Astron. Astrophys. 323 739 1997 1997A&A...323..739B J/A+A/319/413 : ROSAT detected quasars. I. (Brinkmann+ 1997) QSOs X-ray sources galaxies: active quasars: general radio X-rays: general We present the broad band, radio - to - X-ray, properties of a large sample of mostly previously optically unidentified radio-loud X-ray sources from the correlation of a ROSAT All-Sky Survey source list with the 5GHz Green Bank Survey of the northern sky (RGB sample) which is one of the largest well-defined flux-limited surveys of AGN ever obtained. Further, the RGB pushes 1-2 orders of magnitude deeper in both X-ray and radio flux compared to previous unbiased wide-area AGN surveys. Follow up VLA observations of the candidate objects yielded positions with arcsec accuracy which were used to find optical counterparts to the sources from digitized POSS plates. The sources are divided into three classes according to the positional offset between the X-ray and radio candidates and the spatial resolution of the radio observations, reflecting the various degrees of confidence about the correctness of the proposed association. Although the nature of the sources as well as their redshifts remain to be determined in spectroscopic follow up observations, the derived flux ratios lead to the conclusion that the majority of them are quasars. Hardly any correlations could be found between different source parameters, possibly due to the fact that most of the objects are found in a relatively small flux range near the sensitivity limit of the radio catalogue. The majority of the new RGB sources have broad-band properties between those of traditional radio-selected and X-ray selected AGN. There is no bimodal distribution in the radio-loudness distribution, and the traditional division between radio-quiet and radio-loud AGN may not be warranted.
ROSAT
DELTA(VLA-RASS)<40" unidentified RGB sources 40"<DELTA(VLA-RASS)<100" unidentified RGB sources DELTA(VLA-RASS)<100" unidentified RGB sources, low resolution data ROSAT ROSAT name --- RAh VLA right ascension (J2000.0) h RAm VLA right ascension (J2000.0) min RAs VLA right ascension (J2000.0) s DEd VLA declination(J2000.0) deg DEm VLA declination(J2000.0) arcmin DEs VLA declination(J2000.0) arcsec DXrad Angular separation of the VLA radio source and the X-ray source arcsec fr 5GHz VLA flux density from L97 number=1 L97 : Laurent-Muehleisen S.A., Kollgaard R.I., Ryan P.J., et al., 1997A&AS..122..235L mJy FX 0.1 - 2.4 keV X-ray flux 10-15W/m2 e_FX rms uncertainty on FX 10-15W/m2 Gamma X-ray photom index --- e_Gamma Error in Gamma (lower limit) --- E_Gamma Error in Gamma (upper limit) --- Emag E magnitude of the closest optical counterpart from digitized POSS plates (blank: no plate is available) mag n_Emag e: empty fields --- clE [-1/2] Optical classification number=2 -1 = stellar 0 = noise 1 = non-stellar 2 = possible blend --- Omag O magnitude of the closest optical counterpart from digitized POSS plates (blank: no plate is available) mag n_Omag e: empty fields --- clO [-1/2] Optical classification --- DVLAOpt Positional difference between the VLA source and the optical object arcsec E *: the radio source has been re-observed with the Effelsberg telescope (Reich et al., in prep.) --- Notes Notes number=3 Identifications along with a reference are given if the object has been identified after the publication of Brinkmann et al., 1995A&AS..109..147B i = identified as AGN, but as yet no classification available b = BL Lac object q = quasar g = galaxy --- r_Notes References number=4 References: BA = N.Bade, private communication HO = Hook et al. (1996MNRAS.282.1274H) LG = Law-Green et al. (1995MNRAS.274..939L) LM = Laurent-Muehleisen (1996, PhD thesis, Penn State University) MA = Marcha et al. (1996MNRAS.281..425M) NA = Nass et al. (1996A&A...309..419N) NED = Identification from NASA/IPAC extragalactic database PE = Perlman et al. (1996ApJS..104..251P) WA = Wagner et al. (in prep.) ZH = Zhang et al. (in prep.) XIE = Xie et al. (in prep.) --- Previously unidentified RGB sources: VLA empty fields ROSAT ROSAT name --- RAh X-ray ascension (J2000) h RAm X-ray ascension (J2000) min RAs X-ray ascension (J2000) s DEd X-ray declination (J2000) deg DEm X-ray declination (J2000) arcmin DEs X-ray declination (J2000) arcsec DXrad Angular separation of the 87GB radio source and the X-ray source arcsec FX 0.1-2.4 keV X-ray flux 10-15W/m2 e_FX 1 sigma statistical error to the X-ray flux 10-15W/m2 Gamma X-ray photon index assuming Galactic absorption --- e_Gamma Photon index lower 1 sigma error --- E_Gamma Photon index upper 1 sigma error --- log(NH) log (Galactic N_H) [cm-2] F5GHz 87GB 5GHz radio flux in Jy Jy Comm Comment on possible source identification --- tables.tex LaTeX version of the table1-3 Patricia Bauer CDS 1997 Feb 06 Joachim Siebert <jos@rosat.mpe-garching.mpg.de> J_A+A_323_739.xml Is the Sun located near the corotation circle? J/A+A/323/775 J/A+A/323/775 Cepheids radial velocities and coordinates Is the Sun located near the corotation circle? Yu N Mishurov I A Zenina A K Dambis A M Mel'nik A S Rastorguev Astron. Astrophys. 323 775 1997 1997A&A...323..775M Radial velocities Cepheids Galaxy: kinematics and dynamics Galaxy: structure The line-of-sight velocity field of Cepheids was analysed in terms of a disk galaxy model perturbed by spiral density waves in order to estimate the parameters of the galactic rotation curve and the free parameters of density waves. It was shown that: 1) the Sun is located near the corotation circle because the angular rotation velocity of the Galaxy {OMEGA}_{sun}_=~26.0km/s/kpc (Kerr & Lynden-Bell, 1986MNRAS.221.1023K; Dambis, Mel'nik & Rastorguev, 1995AL.....21..291D) is close to that of the spiral pattern {OMEGA}_p_=~28.1+/-2.0km/s/kpc and the corotation radius R_c_=~7. 2+/-1.3kpc (we adopt the galactocentric distance of the Sun R_{sun}_=~7.5kpc); 2) the spiral pitch angle i=~-6.8+/-0.7{deg}; 3) the Sun is at the spiral wave phase {chi}_{sun}_=~290+/-16{deg}; 4) Oort's constant A=~20.9+/-1.2km/s/kpc; the second term in the expansion of the galactic rotation velocity is R_{sun}_^{OMEGA}_{sun}_^=~13.3+/-3.1km/s/kpc^2^.
Cepheids radial velocities and galactic coordinates No Running number --- Star Star's name --- Const Constellation --- GLON Galactic longitude deg GLAT Galactic latitude deg Period Pulsation period d Dist Distance of star from the Sun kpc RV Radial (line-of-sight) velocities of star km/s e_RV Standard errors of radial velocities km/s r_RV References number=1 Radial velocities are taken from : GSRS - Gorynya et al. (1996AL.....22..198G) DMR - Dambis et al. (1995AL.....21..291D) PMB - Pont et al. (1994A&A...285..415P) CC - Caldwell & Coulson (1987AJ.....93.1090C) --- Patricia Bauer CDS 1996 Nov 21 Yu. N. Mishurov <mishurov@phys.rnd.runnet.ru> J_A+A_323_775.xml The variations of the Bp star HD 137509 J/A+A/323/881 J/A+A/323/881 Variations of HD 137509 The variations of the Bp star HD 137509 G Mathys T Lanz Astron. Astrophys. 323 881 1997 1997A&A...323..881M Photometry, Geneva Stars, Bp stars: chemically peculiar stars: individual (HD 137509) stars: magnetic fields stars: rotation A refined value P=(4.4916+/-0.0002) d is derived for the rotation period of the Bp star HD 137509, from the simultaneous consideration of photometric data recorded in the Geneva system and of measurements of the mean longitudinal magnetic field and of the crossover. The photometric data are given in Table 1. For a description of the Geneva photometric system, see e.g. <GCPD/13>
HD 137509 15 31 27.0 -71 03 43
Visual magnitudes and colour indices of HD 137509 in the Geneva photometric system HJD Heliocentric Julian Date of observation d Q Photometric weight Q (Rufener 1988, Cat. <II/169>) --- [V] Geneva [V] magnitude mag P Photometric weight P (Rufener 1988, Cat. <II/169>) --- [U-B] Geneva [U-B] index mag [V-B] Geneva [V-B] index mag [B1-B] Geneva [B1-B] index mag [B2-B] Geneva [B2-B] index mag [V1-B] Geneva [V1-B] index mag [G-B] Geneva [G-B] index mag G. Mathys ESO, Chile Patricia Bauer CDS 1997 Jan 24 Gautier Mathys <gmathys@eso.org> J_A+A_323_881.xml Eclipsing binaries with candidate CP stars. I. Parameters of the systems HD 143654, HD 184035 and HD 185257 J/A+A/324/137 J/A+A/324/137 Eclipsing binaries with candidate CP stars Eclipsing binaries with candidate CP stars. I. Parameters of the systems HD 143654, HD 184035 and HD 185257 P North M Studer M Kunzli Astron. Astrophys. 324 137 1997 1997A&A...324..137N J/A+AS/111/41 : Photometry of magnetic CP stars (North+, 1995) Rufener F., 1988, "Catalogue of stars measured in the Geneva Observatory Photometric system", 4th Edition, Geneva Observatory (Cat. <II/169>) Binaries, eclipsing Binaries, spectroscopic Photometry, Geneva binaries: eclipsing binaries: spectroscopic stars: chemically peculiar stars: early-type stars: early-type stars: fundamental parameters stars: individual (HD 143654, HD 184035, HD 185257) Photometry in the Geneva systems and radial velocities are used to determine the fundamental parameters of three eclipsing binaries, two of which having been classified as chemically peculiar and the third having relatively narrow lines. For a description of the Geneva photometric system, see e.g. <GCPD/13>
HD 143654 TV Nor 16 04 09.1 -51 32 40 HD 184035 V4089 Sgr 19 34 08.3 -40 02 05 HD 185257 V4090 Sgr 19 39 55.3 -39 25 57
Photometry of HD 143654 Photometry of HD 184035 Photometry of HD 185257 HJD Heliocentric Julian date d Q Photometric Q weight (Rufener 1988, Cat. <II/169>) --- Vmag Magnitude in the visible mag P Photometric P weight (Rufener 1988, Cat. <II/169>) --- [U-B] Geneva [U-B] index mag [V-B] Geneva [V-B] index mag [B1-B] Geneva [B1-B] index mag [B2-B] Geneva [B2-B] index mag [V1-B] Geneva [V1-B] index mag [G-B] Geneva [G-B] index mag Patricia Bauer CDS 1997 Feb 19 Pierre North <Pierre.North@obs.unige.ch> J_A+A_324_137.xml Theory of motion and ephemerides of Hyperion J/A+A/324/366 J/A+A/324/366 Theory of motion & ephemerides of Hyperion Theory of motion and ephemerides of Hyperion L Duriez A Vienne Astron. Astrophys. 324 366 1997 1997A&A...324..366D Ephemerides Planets celestial mechanics, stellar dynamics ephemerides planets and satellites: individual (Hyperion) In this paper, we present a new theory of motion for Hyperion, defined like in TASS1.6 for the other Saturn's satellites (Vienne & Duriez, 1995A&A...297..588V), by the osculating saturnicentric orbital elements referred to the equatorial plane of Saturn and to the node of this plane in the mean ecliptic for J2000.0. These elements are expressed as semi-numerical trigonometric series in which the argument of each term is given as an integer combination of 7 natural fundamental arguments (Table 3). These series (Tables 4 to 7) collect all the perturbations caused by Titan on the orbital elements of Hyperion, whose amplitudes are larger than 1km in the long-period terms and than 5km in the short-period ones. Taking also account of the perturbations from other satellites and Sun (Table 8), these series have been fitted to 8136 Earth-based observations of Hyperion in the interval [1874-1985]. The resulting series allows to produce new ephemerides for Hyperion, which have been compared to those previously given by Taylor (1992A&A...265..825T): Using the same set of observations and the same way to weight them, the root mean square (o-c) residual of the present theory is 0.156-arcseconds while the ephemerides of Taylor gives 0.203-arcseconds.
Fundamental arguments of the theory Num Number of the argument --- Arg Argument, see note number=1 psi: Synodic argument between Titan and Hyperion tau: argument of the libration pi7: longitude of the proper pericentre of Hyperion pi6: longitude of the proper pericentre of Titan Om7: longitude of the proper node of Hyperion Om6: longitude of the proper node of Titan Om0: longitude of the node of the invariable plane Each argument is (Freq * t + Phas) where: t = Julian Date - 2451545.0 --- Freq Frequency rad/d Phas Phase rad Per Period d </tableLink> <tableLink xlink:href="table6"> <title>Series for element z of Hyperion Series for element zeta of Hyperion Num Number of the term --- Ampl Amplitude rad N1 Argument number=1 The argument of each term has to be computed as: N1*psi + N2*tau + N3*pi7 + N4*pi6 + N5*Om7 + N6*Om6 + N7*Om0 where psi, tau, pi7, pi6, Om7, Om6, Om0 are given in table3. This is the argument of a cosine in table4, of a sine in table5 and of a complex exponential in table6 and table7 --- N2 Argument number=1 The argument of each term has to be computed as: N1*psi + N2*tau + N3*pi7 + N4*pi6 + N5*Om7 + N6*Om6 + N7*Om0 where psi, tau, pi7, pi6, Om7, Om6, Om0 are given in table3. This is the argument of a cosine in table4, of a sine in table5 and of a complex exponential in table6 and table7 --- N3 Argument number=1 The argument of each term has to be computed as: N1*psi + N2*tau + N3*pi7 + N4*pi6 + N5*Om7 + N6*Om6 + N7*Om0 where psi, tau, pi7, pi6, Om7, Om6, Om0 are given in table3. This is the argument of a cosine in table4, of a sine in table5 and of a complex exponential in table6 and table7 --- N4 Argument number=1 The argument of each term has to be computed as: N1*psi + N2*tau + N3*pi7 + N4*pi6 + N5*Om7 + N6*Om6 + N7*Om0 where psi, tau, pi7, pi6, Om7, Om6, Om0 are given in table3. This is the argument of a cosine in table4, of a sine in table5 and of a complex exponential in table6 and table7 --- N5 Argument number=1 The argument of each term has to be computed as: N1*psi + N2*tau + N3*pi7 + N4*pi6 + N5*Om7 + N6*Om6 + N7*Om0 where psi, tau, pi7, pi6, Om7, Om6, Om0 are given in table3. This is the argument of a cosine in table4, of a sine in table5 and of a complex exponential in table6 and table7 --- N6 Argument number=1 The argument of each term has to be computed as: N1*psi + N2*tau + N3*pi7 + N4*pi6 + N5*Om7 + N6*Om6 + N7*Om0 where psi, tau, pi7, pi6, Om7, Om6, Om0 are given in table3. This is the argument of a cosine in table4, of a sine in table5 and of a complex exponential in table6 and table7 --- N7 Argument number=1 The argument of each term has to be computed as: N1*psi + N2*tau + N3*pi7 + N4*pi6 + N5*Om7 + N6*Om6 + N7*Om0 where psi, tau, pi7, pi6, Om7, Om6, Om0 are given in table3. This is the argument of a cosine in table4, of a sine in table5 and of a complex exponential in table6 and table7 --- Per Period d Solar and short period perturbations of Hyperion Ser Element of Hyperion number=1 p7 : perturbation of element p of Hyperion (series in cosine) q7 : perturbation of element q of Hyperion (series in sine) z7 : perturbation of element z of Hyperion (series in complex exponential) zt7: perturbation of zeta of Hyperion (series in complex exponential) The argument of each term is: (Freq * t + Phas), where: t = Julian Date - 2451545.0 --- Ampl Amplitude rad Freq Frequency rad/d Phas Phase rad Per Period d tables.tex *Tables 3 to 8 in plain TeX format in the same form exactly as the corresponding tables published in A&A Patricia Bauer CDS 1997 Mar 06 L. Duriez <duriez@gat.univ-lille1.fr> J_A+A_324_366.xml Chemical composition of six K supergiants in the Small Magellanic Cloud. J/A+A/324/435 J/A+A/324/435 Chemical composition of six K supergiants in the SMC Chemical composition of six K supergiants in the Small Magellanic Cloud. V Hill Astron. Astrophys. 324 435 1997 1997A&A...324..435H Abundances Stars, supergiant galaxies: abundances Magellanic Clouds stars: abundances supergiants A sample of six SMC cool stars (K supergiants) are analysed by high resolution spectroscopy in order to investigate their chemical content, which should reflect that of the current interstellar medium within the SMC. The abundance of Na, Al, {alpha}-elements, Fe peak and heavy elements are derived through an LTE analysis of the lines, compared to a Galactic "standard" (the well-studied K giant Arcturus) and discussed in terms of chemical evolution of the SMC. The following results were obtained: 1. All the stars from this sample are metal deficient ([Fe/H] ranges from -0.59 to -0.89dex). The abundance varies little from star-to-star (0.10dex rms, comparable with the expected error due to uncertainties on the effective parameters of the stars), in agreement with the very small chemical composition variations among the H II regions within the SMC found by Pagel et al. (1978MNRAS.184..569P). 2. Sodium is not strongly enhanced in these stars, and the star-to-star scatter is larger than expected. 3. At variance with metal-poor stars in our Galaxy, the so-called {alpha}-elements do not seem to be enhanced. 4. Nickel displays a noticeable depletion with respect to iron ([Ni/Fe]=~-0.3dex), at variance with what is found in the SMC F supergiants and in Arcturus. 5. Except for PMMR 144, the s and r process elements heavier than Ba are enhanced in all of our stars by =~+0.4dex.
PMMR 23 SkKM 36 00 48.8 -73 28 PMMR 27 SkKM 43 00 49.2 -73 14 PMMR 48 SkKM 79 00 51.9 -72 12 PMMR 102 SkKM 191 00 59.8 -72 21 PMMR 144 SkKM 250 01 03.3 -72 07 PMMR 145 SkKM 248 01 03.3 -72 40
Lines used in the analysis Lambda Central wavelength of the line 0.1nm Element Name of the element --- n_Element Degree of ionization 1 for neutral, 2 for ionized species --- Pext Excitation potential of the line eV log(gf) Line transition probability in log scale --- EW23 Equivalent width of the line for star PMMR23 mA n_EW23 Note number=1 Asterisks means that the corresponding abundance was determined by fitting the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. --- [X/H]23 Abundance ([X/H]) for PMMR23 Sun EW27 Equivalent width of the line for star PMMR27 mA n_EW27 Note number=1 Asterisks means that the corresponding abundance was determined by fitting the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. --- [X/H]27 Abundance ([X/H]) for PMMR27 Sun EW48 Equivalent width of the line for star PMMR48 mA n_EW48 Note number=1 Asterisks means that the corresponding abundance was determined by fitting the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. --- [X/H]48 Abundance ([X/H]) for PMMR48 Sun EW102 Equivalent width of the line for star PMMR102 mA n_EW102 Note number=1 Asterisks means that the corresponding abundance was determined by fitting the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. --- [X/H]102 Abundance ([X/H]) for PMMR102 Sun EW144 Equivalent width of the line for star PMMR144 mA n_EW144 Note number=1 Asterisks means that the corresponding abundance was determined by fitting the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. --- [X/H]144 Abundance ([X/H]) for PMMR144 Sun EW145 Equivalent width of the line for star PMMR145 mA n_EW145 Note number=1 Asterisks means that the corresponding abundance was determined by fitting the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line. --- [X/H]145 Abundance ([X/H]) for PMMR145 Sun Patricia Bauer CDS 1996 Sep 27 J_A+A_324_435.xml Core velocity dispersions for 25 Galactic and 10 old Magellanic globular clusters J/A+A/324/505 J/A+A/324/505 Core velocity dispersions of globular clusters Core velocity dispersions for 25 Galactic and 10 old Magellanic globular clusters P Dubath G Meylan M Mayor Astron. Astrophys. 324 505 1997 1997A&A...324..505D Clusters, globular Radial velocities Velocity dispersion galaxies: star clusters globular clusters: general Magellanic Clouds stars: kinematics techniques: radial velocities We present, for 25 Galactic and 10 old Magellanic globular clusters, projected velocity dispersion ({sigma}_p_) measurements obtained by applying a cross-correlation technique to integrated-light spectra. In order to understand and estimate the statistical errors of these measurements due to small numbers of bright stars dominating the integrated light, we provide an extensive discussion based on detailed numerical simulations. These errors are smaller if the integration area is larger and/or the cluster concentration higher. The simulations show that measurements are reliable when the integrated light within the integration area is brighter than a given magnitude. The statistical errors on the {sigma}_p_ measurements of Magellanic globular clusters are small because of a physically large integration area, whereas they can be important for measurements carried out over small central areas in Galactic clusters. The present observational results are used to outline a few characteristics of the globular cluster fundamental plane. In this respect, the old Magellanic globular clusters appear similar to the Galactic clusters.
Radial velocities and core velocity dispersions Loc Localication (Gal, LMC or SMC) --- Obs Observation number --- NGC NGC number --- HRV Derived heliocentric radial velocity km/s e_HRV rms uncertainty on HRV km/s sigCCF Standard deviation of the cross-correlation function (CCF) km/s e_sigCCF rms uncertainty on sigCCF km/s Depth Relative depth of the CCF % S/N Signal-to-noise ratio of the spectrum --- eps Uncertainty epsilon of HRV and sigCCF due to the spectrum noise km/s sigref Value used for the intrinsic standard deviation from the standard CCFs km/s e_sigref rms uncertainty on sigref km/s sigpObs Observed cluster core projected velocity dispersion km/s E_sigpObs Error in sigpObs (upper limit) due to the instrumental error and to the spectrum noise km/s e_sigpObs Error in sigpObs (lower limit) due to the instrumental error and to the spectrum noise km/s StatErru Statistical error (upper limit) due to the small sample of bright stars observed through the slit km/s u_StatErru Uncertainty flag on StatErru --- StatErrl Statistical error (lower limit) due to the small sample of bright stars observed through the slit km/s sigp Calculated cluster core projected velocity dispersion number=1 sigp includes the contribution from the statistical error simulations km/s E_sigp Error in sigp (upper limit) number=2 Uncertainty, including the contribution from the statistical error km/s u_E_sigp Uncertainty flag on E_sigp --- e_sigp Error in sigp (lower limit) number=2 Uncertainty, including the contribution from the statistical error km/s Patricia Bauer CDS 1997 Jan 20 Pierre Dubath <Pierre.Dubath@obs.unige.ch> J_A+A_324_505.xml Deep UVBRI photometry in IC 348 J/A+A/324/549 J/A+A/324/549 Deep UVBRI photometry in IC 348 Deep UVBRI photometry in IC 348 E Trullols C Jordi Astron. Astrophys. 324 549 1997 1997A&A...324..549T Clusters, open Photometry, UBVRI Hertzsprung-Russell (HR diagram) open clusters and associations: individual (IC 348) stars: fundamental parameters stars: pre-main sequence Table3 contains UBVRI-CCD photometry for the 123 observed stars in the nucleus of IC 348 open cluster. Magnitude and colours are given with their corresponding errors. Column "N" gives the number of observations. Spectral types and cross-identifications with other catalogues are given in note file. Table5 contains adopted reddening solution for the brightest members in IC 348
IC 348 03 44.5 +32 17
UBVRI-CCD photometry for the 123 observed stars in the nucleus of IC 348 open cluster ID Sequential identification number --- x x-CCD coordinate number=1 x increases from east to west, y from north to south. pix y y-CCD coordinate number=1 x increases from east to west, y from north to south. pix RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V color index mag e_B-V rms uncertainty on B-V mag U-B U-B color index mag e_U-B rms uncertainty on U-B mag V-R V-R color index mag e_V-R rms uncertainty on V-R mag V-I V-I color index mag e_V-I rms uncertainty on V-I mag o_Vmag Number of observations --- member " " non-member; "M" member --- Adopted reddening solution for the brightest members ID Sequential identification number --- E(B-V) Colour excess mag (B-V)0 Intrinsic colour mag Av Visual absorption mag V0 Intrinsic visual magnitude mag N Total number of reddening solutions --- Cross-identifications with other catalogues and spectral types ID Sequential identification number --- Names Other names --- SpType Spectral type --- E. Trullols Universitat Politecnica de Catalunya 1997 Jan 07 Carme Jordi <carme@facjn0.am.ub.es> J_A+A_324_549.xml Complex variability pattern in NGC 4151. I. Sequences on the line-continuum diagram J/A+A/324/904 J/A+A/324/904 NGC 4151 line-continuum diagram sequences Complex variability pattern in NGC 4151. I. Sequences on the line-continuum diagram Yu F Malkov V I Pronik S G Sergeev Astron. Astrophys. 324 904 1997 1997A&A...324..904M Galaxies, Seyfert Galaxies, spectra galaxies: active galaxies: emission lines galaxies: individual (NGC 4151) galaxies: nuclei galaxies: Seyfert We present the first results of an 8-year spectroscopic monitoring of the Seyfert 1.5 galaxy NGC 4151 carried out with a CCD spectrograph at the 2.6-m Shajn Telescope of the Crimean Astrophysical Observatory in 1988-1995. Total of 202 H{ alpha} region spectra and 154 H{beta} region spectra have formed the data set. A ll spectra were calibrated in flux using the narrow emission lines which were as summed to be constant over the duration of the monitoring program.
NGC 4151 12 10 32.5 +39 24 21
Cassegrain H-alpha region fluxes (not corrected for seeing effects) JD Average Julian Date for a night --- Nspect Number of averaged individual spectra --- F635nm Continuum flux density at 635.0 nm 10-13mW/m2/nm F681nm Continuum flux density at 681.5 nm 10-13mW/m2/nm SHalpha Integrated H-alpha line flux 10-11mW/m2 Cassegrain H-beta region fluxes (not corrected for seeing effects) JD Average Julian Date for a night --- Nspect Number of averaged individual spectra --- F512nm Continuum flux at 512.0 nm 10-13mW/m2/nm SHbeta Integrated H-beta line flux 10-12mW/m2 SHeII Integrated HeII 4686 line flux 10-12mW/m2 Nasmyth H-alpha region fluxes (corrected for seeing effects) JD Average Julian Date for a night --- Nspect Number of averaged individual spectra --- Seeing Seeing arcsec F623nm Continuum flux at 623.0 nm 10-13mW/m2/nm F691nm Continuum flux at 691.0 nm 10-13mW/m2/nm SHalpha Integrated H-alpha line flux 10-11mW/m2 Nasmyth H-beta region fluxes (corrected for seeing effects) JD Average Julian Date for a night --- Nspect Number of averaged individual spectra --- Seeing Seeing arcsec F448mn Continuum flux at 448.0 nm 10-13mW/m2/nm F512nm Continuum flux at 512.0 nm 10-13mW/m2/nm SHbeta Integrated H-beta line flux 10-12mW/m2 SHeII Integrated HeII 4686 line flux 10-12mW/m2 S4540 Integrated 4540 feature flux 10-12mW/m2 figure3.ps Seeing correction parameters phi and G for the line and continuum fluxes measured in Nasmyth spectra Patricia Bauer CDS 1997 Feb 26 Yuri Malkov <malkov@crao.crimea.ua> J_A+A_324_904.xml HST observations of Blue Stragglers stars in the core of the globular cluster M3 J/A+A/324/915 J/A+A/324/915 Blue stragglers in M3 HST observations of Blue Stragglers stars in the core of the globular cluster M3 F R Ferraro B Paltrinieri F Fusi Pecci C Cacciari B Dorman R T Rood R Buonanno C E Corsi D Burgarella M Laget Astron. Astrophys. 324 915 1997 1997A&A...324..915F Clusters, globular Photometry, ultraviolet Stars, blue blue stragglers globular clusters: individual (M 3) stars: Population II The core of the Galactic Globular Cluster M 3 (NGC 5272) has been observed with the WFPC2 through the filters F255W, F336W, F555W, and F814W. Using these observations along with a thorough reanalysis of earlier catalogs, we have produced a catalog of blue straggler stars (BSS) spanning the cluster. Earlier studies and the fainter part of our sample suffer severe selection biases. Our analysis is based on a more reliable bright global sample of 122 BSS. We confirm earlier suggestions that the radial BSS distribution in M 3 is bimodal. It is strongly peaked in the center, has a clear dip 100-200" from the center, and rises again at larger radii. The observed distribution agrees with the dynamical model of Sigurdsson et al. (1994ApJ...431L.115S) which takes into account both star collisions and merging of primordial binaries for the origin of BSS. The observed luminosity functions of BSS in the inner and outer parts of the cluster are different. Interpreting these using the models of Bailyn & Pinsonneault (1995ApJ...439..705B), we suggest that the BSS in the inner cluster are formed by stellar collisions and those in the outer cluster from merging primordial binaries.
HST M 3 NGC 5272 13 42.2 +28 23
V,I,U,UV(F255W) photometry of 72 bright BSS in M 3 V,I,U,UV(F255W) photometry of 99 faint BSS in M 3 Star Star designation (this paper) --- Vmag V magnitude mag Imag I magnitude mag Umag U magnitude mag UVmag UV (F255W) magnitude mag Xpos X coordinate arcsec Ypos Y coordinate arcsec Dist Distance from the cluster center arcsec Global sample of 263 BSS in M3 BSS BSS designation in the global sample --- Name Original (this or previous papers) identification number number=1 HST: Hubble Space Telescope F93: Ferraro et al., 1993AJ....106.2324F S53: Sandage, 1953AJ.....58...61S BHS: Bolte et al., 1993ApJ...408L..89B --- n_Name +: BSS in the global bright sample --- Vmag V magnitude mag Xpos X coordinate arcsec Ypos Y coordinate arcsec Dist Distance from the cluster center arcsec GYBS Identification number in GYBS, 1994AJ....108.1786G --- n_GYBS Note on GYBS number=2 n: BSS candidate is located in the field of view of that survey but was not identified as a BSS o: BSS is located out of the field of view --- BHS Identification number in BHS, 1993ApJ...408L..89B --- n_BHS Note on BHS number=2 n: BSS candidate is located in the field of view of that survey but was not identified as a BSS o: BSS is located out of the field of view --- BPQ Identification number in BPQ, 1995A&A...301..675B --- n_BPQ Note on BPQ number=2 n: BSS candidate is located in the field of view of that survey but was not identified as a BSS o: BSS is located out of the field of view --- F93 Identification number in F93, 1993AJ....106.2324F --- n_F93 Note on F93 number=2 n: BSS candidate is located in the field of view of that survey but was not identified as a BSS o: BSS is located out of the field of view --- Patricia Bauer CDS 1997 Feb 24 F.R. Ferraro <FERRARO@astbo3.bo.astro.it> J_A+A_324_915.xml Red giants in open clusters: VII. Melotte 71 J/A+A/324/91 J/A+A/324/91 Melotte 71 red giants radial velocities Red giants in open clusters: VII. Melotte 71 J -C Mermilliod J J Claria J Andersen M Mayor Astron. Astrophys. 324 91 1997 1997A&A...324...91M J/A+A/299/53 : Part IV. NGC 3680 and IC 4651 (Mermilliod+ 1995) J/A+A/307/80 : Part. V. NGC 2099 (Mermilliod+ 1996) J/A+A/319/481 : Part VI. 10 spectroscopic binaries orbits (Mermilliod+ 1997) Mermilliod & Mayor, Paper I =1989A&A...219..125M Mermilliod et al., Paper II =1989A&AS...79...11M Mermilliod & Mayor, Paper III = 1990A&A...237...61M Mermilliod et al., Paper IV =1995A&A...299...53M Mermilliod et al., Paper V =1996A&A...307...80M Clusters, open Radial velocities Stars, giant binaries: spectroscopic Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Mel 71) New CORAVEL radial-velocity observations and UBV photometry of 24 red giants in the field of the intermediate-age open cluster Mel 71 are analysed for membership and duplicity. The membership of 16 stars is confirmed, one star is a possible member, and 8 spectroscopic binaries have been discovered, all amongst the cluster stars. Four of their orbits have been determined, with periods ranging from 74 to 1627 days. The mean cluster velocity is +50.14+/-0.14 (s.e.)km/s, and the binary frequency is unusually high (8/16=50%). The best isochrone fit to the observed colour-magnitude digram is obtained for logt=9.00 and Z=0.008. However, some discrepancies appear between the observed and predicted locations of the red giant clump.
Melotte 71 07 37 20.2 -12 05 53
*Radial velocity data for Melotte 71 ID Star number --- HJD Heliocentric Julian Date d Comp Component of a double-lined binary --- RV Radial velocity km/s e_RV Error on the radial velocity km/s Patricia Bauer CDS 1997 Jan 13 Jean-Claude Mermilliod <Jean-Claude.Mermilliod@obs.unige.ch> J_A+A_324_91.xml Properties of He-rich stars I. Their evolutionary state and helium abundance J/A+A/324/949 J/A+A/324/949 Properties of He-rich stars I. Properties of He-rich stars I. Their evolutionary state and helium abundance M Zboril P North Yu V Glagolevskij F Betrix Astron. Astrophys. 324 949 1997 1997A&A...324..949Z Stars, peculiar stars: abundances stars: atmospheres stars: chemically peculiar stars: fundamental parameters A determination of the surface gravity and an abundance analysis of helium in a sample of 17 He-rich and 5 normal, reference stars is presented. These results are derived from low resolution CCD spectra, but each star was measured at least 6 times in order to obtain a significant average spectrum for the spectroscopic variables. The helium abundances derived from the models used are very close to 0.1 for normal, reference stars and are larger for the others, clearly indicating the He-rich phenomenon in them. NLTE effects, errors on the microturbulence value or on the surface gravity do not influence the estimated helium abundances. Nevertheless, synthesized Geneva colours are affected by the He-rich peculiarity, especially the [U-B] index which systematically changes by -0.025 mag per 0.1 of He abundance for the coolest stars in the sample. We cannot confirm the correlation between the evolutionary state and the helium abundance reported previously (Zboril et al. 1994, in "International Conference on CP and Magnetic Stars.", Tatranska Lomnica, eds. J. Zverko and J. Ziznovsky, p. 105), although we used a more reliable technique of log(g) determination. All He-rich objects lie within the main sequence: their surface gravities are all inside the range 4.1<logg<4.5, with no more than three objects having logg<4.25. We find a significant spread of helium abundances in this range of surface gravities, from the solar value ~0.1 up to about 0.4. Some of the programme stars (including reference stars) present emission in their Balmer lines and therefore some kind of stellar activity. Strong helium overabundance often coexists with emission and stellar activity.
HD 36485 HR 1851 05 32 00.4 -00 17 04 HD 37017 HR 1890 05 35 21.8 -04 29 38 HD 37479 HR 1932 05 38 47.1 -02 35 40 HD 37776 BD-01 1005 05 40 56.3 -01 30 26 HDE 260858 BD+12 1223 06 37 46.6 +12 46 05 HDE 264111 HD 264111 BD+04 1447 06 47 53.8 +04 40 01 CoD-27 3748 SAO 173185 07 12 02.2 -27 43 05 HD 56139 HR 2749 07 14 48.7 -26 46 22 HD 58260 CD-36 3578 07 23 19.6 -36 20 25 HD 60344 CD-23 5673 07 33 02.1 -23 56 03 HD 64740 HR 3089 07 53 03.7 -49 36 47 HD 66522 CD-50 3111 08 01 35.1 -50 36 21 HD 68450 HR 3219 08 11 01.6 -37 17 32 CoD-46 4639 CPD-46 3093 08 49 39.7 -46 50 51 HD 92938 HR 4196 10 42 14.2 -64 27 59 HD 96446 CD-59 3544 CPD-59 3038 11 06 05.8 -59 56 59 CPD-62 2124 LSS 2394 11 35 37.6 -63 15 54 HD 105435 HR 4621 12 08 21.6 -50 43 20 HD 108483 HR 4743 12 28 02.5 -50 13 49 HD 110879 HR 4844 12 46 17.2 -68 06 28 HD 121790 HR 5249 13 58 40.8 -44 48 11 HD 122980 HR 5285 14 06 02.8 -41 10 45 HD 124448 CD-45 9033 14 14 58.5 -46 17 19 HD 133518 CD-51 8745 15 06 55.9 -52 01 47
Journal of the spectroscopic observations Name Star name number=1 The stars HD 105435 and HD 121790 are rotational velocity standards from Slettebak et al., 1975ApJS...29..137S --- HJD Heliocentric Julian date number=2 The epochs are heliocentric Julian dates corresponding to the middle of the exposure. d Texp Exposure time s table1.tex LaTeX version of the table table1.ps Postscript version of the table Patricia Bauer CDS 1997 Feb 27 Pierre North <Pierre.North@obs.unige.ch> J_A+A_324_949.xml Properties and nature of Be stars. 17. V360 Lac = HD 216200 is a B3e + F9IV: binary J/A+A/324/965 J/A+A/324/965 UBV photometry of V360 Lac Properties and nature of Be stars. 17. V360 Lac = HD 216200 is a B3e + F9IV: binary G Hill P Harmanec K Pavlovski H Bozic P Hadrava P Koubsky J Ziznovsky Astron. Astrophys. 324 965 1997 1997A&A...324..965H Binaries, spectroscopic Photometry, UBV Stars, Be binaries: eclipsing binaries: spectroscopic stars: emission-line, Be stars: fundamental parameters stars: individual (V360 Lac) An analysis of an extensive collection of photometric and spectroscopic observations of the little studied bright Be star V360 Lac lead to the following main conclusions: (1) V360 Lac is a binary system consisting of a B3e primary and a F9IV secondary which probably fills the Roche lobe and losses mass towards the primary. Radial-velocity curves of both components were obtained. (2) The light variations arise from superposition of variations on at least three time scales: phase-locked orbital brightness and colour changes with two minima; sinusoidal variation with a 322.24^d^ period and low-amplitude rapid changes with a possible period of 1.6738^d^. (3) A tentative solution of the B and V light curves which assumes the semi-detached configuration and presence of a disk around the primary, combined with the orbital solution, leads to preliminary basic physical elements of the system which are consistent with the radiative properties of the binary components.
V360 Lac 14 Lac HD 216200 22 50 21.7 +41 57 13
V360 Lac: individual homogenized Johnson UBV observations from several stations HJD Heliocentric Julian date d w weight of the data point --- Vmag Johnson V magnitude mag Bmag Johnson B magnitude mag Umag Johnson U magnitude mag B-V Johnson B-V index mag U-B Johnson U-B index mag X Air mass of the observation --- dX Air mass difference between var. and comp. --- HD HD number of the comparison star used --- Obs Numerical code identifying sources of data number=1 Individual observing stations are denoted by their numerical codes used in the Ondrejov photometric data archives as follows: 1 ... Hvar 3 ... Skalnate Pleso 5 ... Lowell 10... Kitt Peak National Observatory 13... Mt Kobau 33... Lick 46... Heidelberg 47... Akita --- Patricia Bauer CDS 1997 Mar 07 Petr Harmanec <hec@sunstel.asu.cas.cz> J_A+A_324_965.xml Coronal and chromospheric emission from cool stars in near-simultaneous ROSAT All-Sky Survey and Mount Wilson data J/A+A/325/1115 J/A+A/325/1115 Near-simultaneous ROSAT and Mt Wilson data Coronal and chromospheric emission from cool stars in near-simultaneous ROSAT All-Sky Survey and Mount Wilson data A J M Piters C J Schrijver J H M M Schmitt C Rosso S L Baliunas J Van Paradijs C Zwaan Astron. Astrophys. 325 1115 1997 1997A&A...325.1115P Stars, late-type X-ray sources stars: chromospheres stars: coronae stars: late-type X-rays: stars Table 1 lists near-simultaneous X-ray data and Ca II H&K line-core emission data from the ROSAT All-Sky Survey and from the Mt. Wilson H&K spectrometer, respectively. The stars in this sample are 215 bright F-, G-, and K-type stars. Table 2 lists the derived excess Ca II H&K line-core and the X-ray flux densities for the same stars.
X-ray and Ca II data HD HD number --- B-V B-V (from [1]) --- Bin Information on binarity, See Note number=1 Information on binarity: S: single SB1: single-lined spectroscopic binary SB2: double-lined spectroscopic binary VB: visual binary --- Type Spectral Type (from [1]) --- JDCa Obs. Time Ca II (JD-2444000) d JDX Obs. Time X-ray (JD-2444000) d T(Ca-X) Obs. Time Difference (Ca II - X-ray) d Sval S-value --- e_Sval Uncertainty in S-value --- n_Sval Note on Sval. See Note number=2 Information on the S-value: A: only one measurement, the uncertainty is 2% B: S_val is the S2-value C: S_val is the S1-value blank (and A): S_val is the S1-value if the luminosity class is between IV and V and S_val is the S2-value if the luminosity class is between II to III-IV --- l_Xrate Upper limit for Xrate. See Note number=3 U: the X-ray Count Rate given is a 3 sigma upper limit value (no hardness ratio and uncertainties are given) blank: otherwise --- Xrate X-ray Count Rate ct/s E_Xrate Pos. Uncertainty in Count Rate ct/s e_Xrate Neg. Uncertainty in Count Rate ct/s HR Hardness Ratio --- E_HR Pos. Uncertainty in Hardness Ratio --- e_HR Neg. Uncertainty in Hardness Ratio --- n_Xrate Note on Xrate and HR. See Note number=4 Information on Count Rate and Hardness Ratio: D: Total Count Rate and mean Hardness Ratio of HD26913 + HD26923 or HD201091 + HD201092 E: Count Rate and Hardness Ratio derived from the ROSAT Standard Analysis Software System blank: no additional information --- LogNH Hydrogen Column Density [cm-2] e_LogNH Uncertainty in LogNH [cm-2] Flux densities HD HD number (Cat. <III/135>) --- DFCa Excess CaII surface flux density number=1 DFCa is the logarithmic Ca II H&K line-core emission surface flux density in excess of the minimum flux density derived by Rutten (1987A&A...177..131R) DFCa is expressed in Rutten's arbitrary units (1982A&A...130..353R) (Logarithmic) uncertainties are given in the same units. If the negative uncertainty is missing (left blank), the uncertainty is infinity, meaning that the negative uncertainty in the non-logarithmic value is of the order of the value itself; this occurs when the Ca II flux density is close to the minimum flux density. If no value is given for the excess Ca II surface flux density and the normalized flux density (DRCaII) the calculated Ca II flux density is smaller than the minimum flux density. --- E_DFCa Positive uncertainty in DFCa number=1 DFCa is the logarithmic Ca II H&K line-core emission surface flux density in excess of the minimum flux density derived by Rutten (1987A&A...177..131R) DFCa is expressed in Rutten's arbitrary units (1982A&A...130..353R) (Logarithmic) uncertainties are given in the same units. If the negative uncertainty is missing (left blank), the uncertainty is infinity, meaning that the negative uncertainty in the non-logarithmic value is of the order of the value itself; this occurs when the Ca II flux density is close to the minimum flux density. If no value is given for the excess Ca II surface flux density and the normalized flux density (DRCaII) the calculated Ca II flux density is smaller than the minimum flux density. --- e_DFCa Negative uncertainty in DFCa number=1 DFCa is the logarithmic Ca II H&K line-core emission surface flux density in excess of the minimum flux density derived by Rutten (1987A&A...177..131R) DFCa is expressed in Rutten's arbitrary units (1982A&A...130..353R) (Logarithmic) uncertainties are given in the same units. If the negative uncertainty is missing (left blank), the uncertainty is infinity, meaning that the negative uncertainty in the non-logarithmic value is of the order of the value itself; this occurs when the Ca II flux density is close to the minimum flux density. If no value is given for the excess Ca II surface flux density and the normalized flux density (DRCaII) the calculated Ca II flux density is smaller than the minimum flux density. --- FX Log. X-ray surface flux density number=2 FX is the logarithmic X-ray surface flux density in erg/(s*cm^2). if the uncertainties E_FX and e_F_X is missing (left blank), the surface flux density and the normalized flux density, RX, are upper limit values. [mW/m2] E_FX Positive uncertainty in FX number=2 FX is the logarithmic X-ray surface flux density in erg/(s*cm^2). if the uncertainties E_FX and e_F_X is missing (left blank), the surface flux density and the normalized flux density, RX, are upper limit values. [mW/m2] e_FX Negative uncertainty in FX number=2 FX is the logarithmic X-ray surface flux density in erg/(s*cm^2). if the uncertainties E_FX and e_F_X is missing (left blank), the surface flux density and the normalized flux density, RX, are upper limit values. [mW/m2] DRCaII Exc. CaII normalized flux dens. number=1 DFCa is the logarithmic Ca II H&K line-core emission surface flux density in excess of the minimum flux density derived by Rutten (1987A&A...177..131R) DFCa is expressed in Rutten's arbitrary units (1982A&A...130..353R) (Logarithmic) uncertainties are given in the same units. If the negative uncertainty is missing (left blank), the uncertainty is infinity, meaning that the negative uncertainty in the non-logarithmic value is of the order of the value itself; this occurs when the Ca II flux density is close to the minimum flux density. If no value is given for the excess Ca II surface flux density and the normalized flux density (DRCaII) the calculated Ca II flux density is smaller than the minimum flux density. --- RX X-ray normalized flux density number=2 FX is the logarithmic X-ray surface flux density in erg/(s*cm^2). if the uncertainties E_FX and e_F_X is missing (left blank), the surface flux density and the normalized flux density, RX, are upper limit values. --- Note See Note number=3 A: Total FX and RX of HD 26913 + HD 26923 B: Total FX and RX of HD 201091 + HD 201092 --- Patricia Bauer CDS 1997 Jun 09 Ankie Piters <piters@knmi.nl> J_A+A_325_1115.xml A 330-360 GHz spectral survey of G34.3+0.15. II. Chemical modelling. J/A+A/325/1163 J/A+A/325/1163 330-360GHz spectral lines of G 34.3+0.15. II. A 330-360 GHz spectral survey of G34.3+0.15. II. Chemical modelling. T J Millar G H Macdonald A G Gibb Astron. Astrophys. 325 1163 1997 1997A&A...325.1163M J/A+AS/119/333 : 330-360GHz spectral lines of G 34.3+0.15. (Macdonald+, 1996) Interstellar medium ISM: abundances ISM: individual (G34.3+0.15) ISM: molecules Tables 5 and 6 present calculated column densities (in units of molecules per cm^2^) of various species in the ultracompact core (UCC), the compact core (CC) and the halo, together with the total column density and the observed column density where available. Table 5 gives column densities at a time of 3x10^3yrs in the UCC and CC components and at 10^5yrs in the halo. Table 6 gives column densities at a time of 10^4yrs in the UCC and CC components and 10^5yrs in the halo.
GRS 34.3+0.15 18 53 18.4 +01 14 58
*Column densities at 3x10^3^yrs in the UCC and CC components and at 10^5^yrs in the halo. *Column densities at 10^4^yrs in the UCC and CC components and at 10^5^yrs in the halo. Species Chemical species --- N(UCC) Ultracompact core column density cm-2 N(CC) Compact core column density cm-2 N(Halo) Halo column density cm-2 N(Tot) Total column density cm-2 l_N(Obs) Limit flag on N(obs) --- N(Obs) Observed column density cm-2 fig1.ps Evolution of column densities in the ultracompact core fig2.ps Evolution of column densities in the compact core fig3.ps Evolution of column densities in the halo fig5.ps Radial distributions of many molecules fig6.ps Radial distributions of many molecules Tom J. Millar UMIST Patricia Bauer CDS 1997 Jun 12 Tom Millar <tjm@rhea.phy.umist.ac.uk> J_A+A_325_1163.xml Geneva photometry in the young open cluster NGC 6231 J/A+A/325/167 J/A+A/325/167 Geneva photometry in NGC 6231 Geneva photometry in the young open cluster NGC 6231 D Raboud N Cramer P A Bernasconi Astron. Astrophys. 325 167 1997 1997A&A...325..167R J/A+A/315/384 : Binarity among B-stars in NGC 6231 (Raboud, 1996) Braes L.L.E. 1967, Bull. Astr. Inst. Neth. Suppl., 2, 1 =1967BANS....2....1B Raboud D. 1996, A&A, 315, 384 =1996A&A...315..384R, Cat. <J/A+A/315/384> Clusters, open Photometry, Geneva open clusters and associations: individual (NGC 6231) stars: formation stars: pre-main sequence techniques: photometric We present photoelectric (127 stars) and CCD (168 stars) Geneva photometry for the very young open cluster NGC 6231. We have searched for new cluster members out to a distance of ~13arcmin, extending the Seggewiss area (~8arcmin), and we found at least 64 new probable members in this extended field. Differential reddening is clearly measured across the cluster area. We determine the cluster distance (1800pc) and age (3.8+/-0.6x10^6^yr). The probable presence of pre-main sequence stars and the consequence of this population on the cluster formation history is analysed. We also found that the O8.5III star S161 is a long term variable and we present its light curve extending over more than 20 years. Finally we discuss the existence of Ap stars in the cluster. For a description of the Geneva photometric system, see e.g. <GCPD/13>
NGC 6231 16 54.2 -41 48
</tableLink> </tableLinks> <fields> <field> <name>Number</name> <definition>Star number</definition> <units>---</units> </field> <field> <name>n_Number</name> <definition>Note on Number <footnote footnoteId="???"> <para>number=1</para> <para>1: CCD measurement</para> </footnote> </definition> <units>---</units> </field> <field> <name>Class</name> <definition>Classification</definition> <units>---</units> </field> <field> <name>u_Class</name> <definition>Uncertainty flag on Class</definition> <units>---</units> </field> <field> <name>Vmag</name> <definition>Apparent V magnitude</definition> <units>mag</units> </field> <field> <name>X</name> <definition>X parameter in Geneva photometry</definition> <units>mag</units> </field> <field> <name>Y</name> <definition>Y parameter in Geneva photometry</definition> <units>mag</units> </field> <field> <name>Z</name> <definition>Z parameter in Geneva photometry</definition> <units>mag</units> </field> <field> <name>Ebv</name> <definition>Colour excess</definition> <units>mag</units> </field> <field> <name>MVmag</name> <definition>Absolute V magnitude</definition> <units>mag</units> </field> <field> <name>U-B</name> <definition>U-B Geneva colour</definition> <units>---</units> </field> <field> <name>B-V</name> <definition>B-V Geneva colour</definition> <units>km/s</units> </field> <field> <name>xpos</name> <definition>x coordinate centered on S289 <footnote footnoteId="???"> <para>number=2</para> <para>1 pix = 1/16.4 arcmin</para> </footnote> </definition> <units>pix</units> </field> <field> <name>ypos</name> <definition>y coordinate centered on S289 <footnote footnoteId="???"> <para>number=2</para> <para>1 pix = 1/16.4 arcmin</para> </footnote> </definition> <units>pix</units> </field> <field> <name>SpT</name> <definition>Estimated photometric spectral type (for table3 and 5) or Rejection criteria (for table4)</definition> <units>---</units> </field> <field> <name>n_Class</name> <definition>Remark on classification. See Note <footnote footnoteId="???"> <para>number=3</para> <para>1: The star could be considered as non-member, following the proper motion values by Braes (1967BANS....2....1B) 2: Likely non-member, following Raboud (1996, Cat. <J/A+A/315/384>)</para> </footnote> </definition> <units>---</units> </field> </fields> </tableHead> <history> <ingest> <creator> <lastName>Raboud</lastName> <affiliation>University of Lausanne</affiliation> </creator> <date> <year>1997</year> <month>Mar</month> <day>7</day> </date> <acknowledgement>Didier Raboud <Didier.Raboud@obs.unige.ch></acknowledgement> </ingest> </history> <identifier>J_A+A_325_167.xml</identifier> </dataset> <dataset subject="astronomy" xmlns:xlink="http://www.w3.org/XML/XLink/0.9"> <title>HI-deficiency in Hickson compact groups of galaxies J/A+A/325/473 J/A+A/325/473 HCG HI-deficiency HI-deficiency in Hickson compact groups of galaxies W K Huchtmeier Astron. Astrophys. 325 473 1997 1997A&A...325..473H VII/85 : Hickson Compact Groups of Galaxies (Hickson 1982) Clusters, galaxy Radio lines galaxies: clusters: general ISM: general We present HI observations of 54 Hickson Compact Groups (HCG) of which 41 have been detected in the 21-cm line of neutral hydrogen. For 13 objects upper limits have been obtained. The integrated M_HI_/L_B_ values of the observed HCGs scatter over a large range of values showing strong HI-deficiencies for a great number of objects.
Observational data HCG HCG number number=1 Individual notes: HCG4 b and a: HI-data for the profiles at the optical velocities of components b and a HCG14 c and a: HI-data for the profiles at the optical velocities of components c and a HCG22, HCG42 and HCG68: data from Huchtmeier (1994A&A...286..389H) HCG41, HCG78: HI data correspond to individual galaxies in the velocity range searched --- m_HCG Multiplicity index on HCG --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec z Optical redshift --- Nspir Total number of spiral galaxies number=2 Total numbers in the brightest three magnitudes --- Ngal Total number of galaxies number=2 Total numbers in the brightest three magnitudes --- LB Blue luminosity number=3 Integrated blue luminosity of all member galaxies later than type E within the velocity interval searched for HI 10+10solLum SHI Measured HI flux Jy.km/s u_SHI Uncertainty flag on SHI --- Peak Observed peak of the line number=4 For non-detections, only the rms noise is shown mJy e_Peak rms uncertainty on Peak mJy HRVHI HI heliocentric radial velocity number=5 Velocity derived from the midpoint of the line at 25% and 20% of the peak km/s e_HRVHI rms uncertainty on HRVHI km/s LW50 Linewidth at a level of 50% of line peak km/s u_LW50 Uncertainty flag on LW50 --- LW25 Linewidth at a level of 25% of line peak km/s u_LW25 Uncertainty flag on LW25 --- LW20 Linewidth at a level of 20% of line peak km/s u_LW20 Uncertainty flag on LW20 --- l_MHI/LB Limit flag on MHI/LB --- MHI/LB Relative HI-content MHI/LB of the group --- *Global parameters of Hickson compact groups of galaxies (Cat. <VII/85>) HCG HCG number number=1 Individual notes: HCG22, HCG42 and HCG68: data from Huchtmeier (1994A&A...286..389H) HCG41, HCG78: HI data correspond to individual galaxies in the velocity range searched --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec z Optical redshift --- HRVHI HI heliocentric radial velocity km/s Dist Assumed distance Mpc LB Blue luminosity number=2 Blue luminosity of all group members later than than type E within the velocity interval of the HI observations 10+10solLum l_MHI Limit flag on HI mass --- MHI Total HI mass 10+9solMass l_MHI/LB Limit flag on MHI/LB --- MHI/LB HI mass to blue luminosity ratio --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Apr 24 Walter Huchtmeier <p083huc@mpifr-bonn.mpg.de> J_A+A_325_473.xml Optical high-resolution spectroscopy of ROSAT detected late-type stars south of the Taurus molecular clouds J/A+A/325/647 J/A+A/325/647 High-resolution spectra south of Taurus Optical high-resolution spectroscopy of ROSAT detected late-type stars south of the Taurus molecular clouds R Neuhauser G Torres M F Sterzik S Randich Astron. Astrophys. 325 647 1997 1997A&A...325..647N Radial velocities Rotaional velocities Stars, late-type stars: formation stars: late-type stars: pre-main sequence X-rays: stars Listed are results from our high-resolution data for all stars in our study area which were listed by either Magazzu et al. (1997A&AS..124..449M) or Alcala et al. (1996A&AS..119....7A), i.e. T Tauri candidates from the ROSAT All-Sky Survey. In table 1, we list all stars for which lithium was found either by Magazzu et al. (1997A&AS..124..449M) or in our CASPEC spectra, as well as two stars identified as wTTS by Alcala et al. (1996A&AS..119....7A). Listed are the designation, number of single-order echelle spectra taken, effective temperatures, projected rotational velocities, mean heliocentric radial velocities with errors, radial velocities in the local standard of rest, and remarks on variability in radial velocity as found in our high-resolution spectra. For comparison, we also list the results on spectral types of the stars (with `e' for H{alpha} emission) as found by Magazzu et al. (1997A&AS..124..449M) (or Alcala et al., 1996A&AS..119....7A) with low- and medium-resolution spectroscopy. In the last two columns, we list the (NLTE) lithium abundance (given on a scale where logN(H)=12) and the lithium excess above the relevant Pleiades upper envelope; upper limits indicate stars where the Magazzu et al. (1997A&AS..124..449M) spectra suffer from either low S/N or low resolution. In table 2, we list all stars where no lithium was detected -- neither by Magazzu et al. (1997A&AS..124..449M) nor in our CASPEC spectra.
ROSAT
High-resolution data for lithium-rich ROSAT source counterparts Name Name of objects number=1 Row 1 to 9: K-type stars with lithium excess south of Taurus: PMS stars younger than 30 million years Row 10 to 18: K-type stars located on lambda Ori with lithium excess: PMS stars younger than 30 million years Row 19 to 33: F8- to G9-type stars with lithium excess: ZAMS stars older than 30 million years Row 34 to 40: Lithium upper limits due to low S/N or low-resolution spectra Row 41 to 56: Stars with lithium, but without lithium excess: ZAMS stars older than 100 million years --- No Number of high-resolution observations --- Teff Effective temperature K vsini Rotational velocity v sin i km/s HRV Heliocentric radial velocity km/s e_HRV Error in radial velocity km/s RVlsr Local-standard-of-rest radial velocity km/s Rem Remarks number=2 SB 1 or 2: single- or double-lined spectroscopic binaries. --- M97 Results from Magazzu et al. (1997A&AS..124..449M) number=3 (N): Listed as "wTTS" in Neuhaeuser et al. (1995A&A...299L..13N) (1): Spectral type given by Alcala et al. (1996A&AS..119....7A), who identified these stars as wTTS. (2): SB as found in our CASPEC spectrum; components NW and SE are separated by 14 arcsec (Magazzu et al., 1997A&AS..124..449M) (3): SB as found by Magazzu et al. (1997A&AS..124..449M), who found lithium in both components; data given here are for the primary, which is much brighter. (4): We have revised EW(Li) down to 0.25 Angstrom from the value given in Magazzu et al. (1997A&AS..124..449M), which apparently was too large due to an incorrect assumption on the continuum level. (5): Classified as a wTTS by N95c, but as a dKe star by Magazzu et al. (1997A&AS..124..449M); we detect lithium in our CASPEC spectrum but not in excess of the Pleiades level, and conclude that this star is a K5 ZAMS star. (6): Magazzu et al. (1997A&AS..124..449M) detected lithium, but did not classify this star as `PMS' or `PMS?'. (7) Lithium data from our high-resolution CASPEC spectra. (8) Orbit known (Torres et al., in preparation). --- NLi log of Lithium abundance N(Li) [Sun] n_NLi Unknown value --- dEW(Li) Lithium excess above ZAMS level 0.1nm n_dEW(Li) Unknown value --- ULdEW(Li) Upper limits on Lithium excess above ZAMS level 0.1nm High-resolution data for ROSAT sources with undetected lithium Name Name of objects --- no Number of high-resolution observations --- Teff Effective temperature K vsini Rotational velocity v sin i km/s ULvsini Upper limit on v sin i km/s HRV Heliocentric radial velocity km/s e_HRV Error in radial velocity km/s RVlsr Local-standard-of-rest radial velocity km/s remarks Remarks number=1 SB 1 or 2: single- or double-lined spectroscopic binaries. If "orbit" is given, then the orbit is known (Torres et al., in prep.) (1): Lines in high-resolution spectra are too broad to obtain reliable data. --- M97 Results from Magazzu et al. (1997A&AS..124..449M) --- Ralph Neuhaeuser MPE Garching Patricia Bauer CDS 1997 Jul 22 Ralph Neuhaeuser <rne@rosat.mpe-garching.mpg.de> J_A+A_325_647.xml B-type pulsators in the open cluster NGC 884 ({chi} Persei) J/A+A/325/987 J/A+A/325/987 UBV magnitude of NGC 884 B-type pulsators B-type pulsators in the open cluster NGC 884 ({chi} Persei) J Krzesinski A Pigulski Astron. Astrophys. 325 987 1997 1997A&A...325..987K Clusters, open Photometry, UBV Stars, Be open clusters and associations: individual (NGC 884, chi Per) stars: emission-line, Be stars: oscillations stars: variables: other (beta Ceph) We present the results of the photometric CCD search for B-type pulsators in the central region of Chi Persei (NGC 884) open cluster. In addition to the two newly-discovered Beta Cephei stars we found 11 other variables in the observed field. The photometric data for them are given in the file 'bmag' and 'vmag' for B and V-filter data, respectively. In addition, we present the new UBV magnitudes for stars in the observed field. This is Table 4 of the paper, available only in electronic form.
Oo 2246 NGC 884 2246 BD+56 572 02 22 02.7 +57 08 25 Oo 2299 NGC 884 2299 BD+56 575 02 22 08.5 +57 07 28 Oo 2088 NGC 884 2088 V506 Per 02 21 43.4 +57 07 32 Oo 2140 NGC 884 2140 02 21 49.9 +57 07 05 Oo 2165 NGC 884 2165 V507 Per 02 21 53.1 +57 09 57 Oo 2227 NGC 884 2227 HD 14443 02 22 00.5 +57 08 43 Oo 2242 NGC 884 2242 02 22 02.5 +57 09 20 Oo 2301 NGC 884 2301 02 22 09.0 +57 07 24 Oo 2311 NGC 884 2311 BD+56 576 02 22 09.6 +57 07 02 Oo 2371 NGC 884 2371 BD+56 578 02 22 17.6 +57 07 25 Oo 2417 NGC 884 2417 HD 14488 02 22 24.2 +57 06 34
B-filter photometry of variable stars U-filter photometry of variable stars V-filter photometry of variable stars HJD Heliocentric Julian day d Oo2246 Differential magnitude for Oo 2246, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2299 Differential magnitude for Oo 2299, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2088 Differential magnitude for Oo 2088, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2140 Differential magnitude for Oo 2140, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2165 Differential magnitude for Oo 2165, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2227 Differential magnitude for Oo 2227, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2242 Differential magnitude for Oo 2242, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2301 Differential magnitude for Oo 2301, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2311 Differential magnitude for Oo 2311, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2371 Differential magnitude for Oo 2371, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag Oo2417 Differential magnitude for Oo 2417, number=1 All magnitude are differential magnitudes in the sense of variable minus comparison, where in all cases the comparison star is the mean magnitude of two comparison stars, Oo 2235 and Oo 2296. mag UBV photometry of stars in the observed field Xpos X coordinate of a star (as in Fig.1) pix Ypos Y coordinate of a star (as in Fig.1) pix Name Star designation, see Note number=1 Star numbers are according to Oosterhoff (1937AnLei..17a...1O) except for those preceded by 'W' or 'VM' for which the designations were taken from Wildey (1964ApJ...139..435W) and Vogt & Moffat (1974VeBoc...2....1V), respectively. --- Vmag V magnitude, see Note number=2 For variable stars we use the following rules in listing their UBV magnitudes: for periodic variables (Oo 2246, 2299, 2371) we list the mean magnitudes, while for the eclipsing binaries (Oo 2301 and 2311) the magnitudes at the phase of maximum light are given. For the remaining 6 variables we give the UBV magnitudes at one, arbitrarily chosen epoch, HJD 2450163.338, i.e., the middle of the night March 19/20, 1996. mag B-V B-V colour index, see Note number=2 For variable stars we use the following rules in listing their UBV magnitudes: for periodic variables (Oo 2246, 2299, 2371) we list the mean magnitudes, while for the eclipsing binaries (Oo 2301 and 2311) the magnitudes at the phase of maximum light are given. For the remaining 6 variables we give the UBV magnitudes at one, arbitrarily chosen epoch, HJD 2450163.338, i.e., the middle of the night March 19/20, 1996. mag U-B U-B colour index, see Note number=2 For variable stars we use the following rules in listing their UBV magnitudes: for periodic variables (Oo 2246, 2299, 2371) we list the mean magnitudes, while for the eclipsing binaries (Oo 2301 and 2311) the magnitudes at the phase of maximum light are given. For the remaining 6 variables we give the UBV magnitudes at one, arbitrarily chosen epoch, HJD 2450163.338, i.e., the middle of the night March 19/20, 1996. --- Patricia Bauer CDS 1997 Oct 16 Andrzej Pigulski, <pigulski@astro.uni.wroc.pl> J_A+A_325_987.xml Photometric versus empirical surface gravities of eclipsing binaries J/A+A/326/1044 J/A+A/326/1044 Eclipsing binaries uvbyHbeta photometry Photometric versus empirical surface gravities of eclipsing binaries C Jordi I Ribas J Torra A Gimenez Astron. Astrophys. 326 1044 1997 1997A&A...326.1044J Binaries, eclipsing Photometry, uvby, beta binaries: eclipsing stars: early-type stars: fundamental parameters stars: late-type Systematic differences in photometric stellar surface gravity determination are studied by means of the comparison with empirical values derived from detached double-lined eclipsing binaries. Photometric gravities were computed using Moon & Dworetsky (1985MNRAS.217..305M) grids based on Kurucz (1979ApJS...40....1K) atmosphere models, and empiric al gravities were taken from Andersen (1991A&ARv...3...91A). Individual Stroemgren colours and {beta} indices of each component of the binary system have to be taken into account to correctly analyze the observed differences. A compilation of data on a sample containing 30 detached double-lined eclipsing binaries with accurate (=~1-2%) determination of mass and radius and available uvbyH_{beta}_ photometric data is also presented. Correction of the differences in terms of T_eff_ and logg for the range 11000K<T_eff_<20000K reduces the mean residuals from 0.13dex to 0.07dex. For the range 7000K<T_eff_<8500K, the consideration of metallicity effects by means of {delta}m_o_ index improves the accuracy from 0.20dex to 0.09dex.
uvbyH{beta} photometry for 30 detached eclipsing binaries Name Identification name (Name, HD, BD) --- m_Name Component: A=primary, B=secondary --- SpType Spectral type --- RAh Right Ascension 2000 (hours) number=4 The coordinates have been added at CDS. h RAm Right Ascension 2000 (minutes) number=4 The coordinates have been added at CDS. min RAs Right Ascension 2000 (seconds) number=4 The coordinates have been added at CDS. s DE- Declination 2000 (sign) number=4 The coordinates have been added at CDS. --- DEd Declination 2000 (degrees) number=4 The coordinates have been added at CDS. deg DEm Declination 2000 (minutes) number=4 The coordinates have been added at CDS. arcmin DEs Declination 2000 (seconds) number=4 The coordinates have been added at CDS. arcsec Vmag Visual apparent magnitude mag e_Vmag Error in Vmag mag (b-y) b-y index mag e_(b-y) Error in b-y mag m1 m1 index ((v-b) - (b-y)) mag e_m1 Error in m1 mag c1 c1 index ((u-v) - (v-b)) mag e_c1 Error in c1 mag beta H{beta} index mag e_beta Error in beta mag logg(emp) Empirical determination of logg number=1 From light and radial velocity curve analysis. Errors in logg(emp) can be found in Andersen (1991A&ARv...3...91A) and range from 0.007 to 0.025dex with a mean value of 0.014dex. [cm/s2] logg(MD) Photometric determination of logg number=2 Photometric determination using MD grids and NSW interpolation. Estimated errors in logg(MD) and Teff(MD) increase from 0.15 to 0.30dex and from 200 to 1200K, respectively, when the temperature increases from 6000 to 20000K [cm/s2] logg(cor) Corrected photometric determination of logg [cm/s2] Teff(MD) Photometric determination of effective temperature number=2 Photometric determination using MD grids and NSW interpolation. Estimated errors in logg(MD) and Teff(MD) increase from 0.15 to 0.30dex and from 200 to 1200K, respectively, when the temperature increases from 6000 to 20000K K Notes Notes number=3 a. Clausen J.V., 1991A&A...246..397C b. Clausen J.V., 1996A&A...308..151C c. Nordstroem B., Johansen K.T., 1994A&A...282..787N d. Nordstroem B., Johansen K.T., 1994A&A...291..777N e. Popper D.M., Andersen J., Clausen J.V., Nordstrom B., 1985AJ.....90.1324P f. Andersen J., Clausen J.V., 1989A&A...213..183A g. Andersen J., Clausen J.V., Nordstrom, B., Reipurth B., 1983A&A...121..271A h. This work i. Gronbech B., Gyldenkerne K., Jorgensen H.E., 1977A&A....55..401G j. Clausen J.V., Gimenez A., 1991A&A...241...98C k. Clausen J.V., Nordstrom B., 1980A&A....83..339C l. Luminosity ratios from Jorgensen H.E., Gyldenkerne K., 1975A&A....44..343J m. Jorgensen H.E., Gronbech B., 1978A&A....66..377J n. Gimenez A., 1994, private communication o. Clausen J.V., Nordstrom B., 1978A&A....67...15C p. Andersen J., Clausen J.V., Gimenez A., 1993A&A...277..439A q. Andersen J., Clausen J.V., Nordstrom B., 1987A&A...175...60A r. Clausen J.V., Gronbech B., 1976A&A....48...49C s. Clausen J.V., Gimenez A., Scarfe C.D., 1986A&A...167..287C t. Andersen J., Clausen J.V., Nordstrom B., 1990A&A...228..365A u. VandenBerg D.A., Hrivnak B.J., 1985ApJ...291..270V v. Clausen J.V., Gyldenkerne K., Gronbech B., 1976A&A....46..205C w. Luminosity ratios from Vaz L.P.R., Andersen J., 1984A&A...132..219V x. Andersen J., Clausen J.V., Nordstrom B., 1984A&A...134..147A y. Clausen J.V., Gyldenkerne K., Gronbech B., 1977A&A....58..121C z. Andersen J., Clausen J.V., Nordstrom B., Popper D.M., 1985A&A...151..329A aa. Clausen J.V., Gronbech B., 1977A&A....58..131C ab. Andersen J., Clausen J.V., Nordstrom B., 1984A&A...137..281A * beta{A} and beta{B} computed from joint beta and beta{Min I} --- Patricia Bauer CDS 1997 May 29 Carme Jordi <carme@facjn0.am.ub.es> J_A+A_326_1044.xml More Light on RV Tau Variables J/A+A/326/1069 J/A+A/326/1069 Abundances in globular clusters More Light on RV Tau Variables S C Russell Astron. Astrophys. 326 1069 1997 1997A&A...326.1069R Abundances Clusters, globular Stars, giant Stars, variable globular clusters: general stars: abundances stars: AGB and post-AGB stars: variables: other Tables 5, 6, and 7 present details of the derived abundances for the stars observed in the globular clusters M2, M13, and M56, respectively. Table 9 gives the measured equivalent widths for the iron lines of the field stars. Table 10 gives the measured equivalent widths for the programme stars of this survey.
M 2 NGC 7089 21 33 29.2 -00 49 23 M 13 NGC 6205 16 41 41.4 +36 27 37 M 56 NGC 6779 19 16 35.4 +30 11 04
Measured Abundances for M2 Star Star Name --- Element Element --- Z Atomic Number --- Solar Solar abundance (H=12) [] Abundance Abundance of star [] sigma Standard deviation of results [] N number of lines used to derive abundance --- Measured Abundances for M13 Measured Abundances for M56 Star Star Name --- Element Element --- Z Atomic Number --- Abundance Abundance of star [] sigma Standard deviation of results [] N Number of lines used to derive abundance --- Equivalent widths for FeI and FeI for standard stars Element Element --- lambda Wavelength 0.1nm EW(HD165195) HD 165195 equivalent width 0.1pm u_EW(HD165195) Uncertainty flag on EW(HD165195) --- EW(BD+302611) BD +30 2611 equivalent width 0.1pm EW(HD204543) HD 204543 equivalent width 0.1pm EW(HD135148) HD 135148 equivalent width 0.1pm u_EW(HD135148) Uncertainty flag on EW(HD135148) --- Equivalent widths for programme stars Element Element --- Z Atomic Number --- lambda Wavelength 0.1nm loggf Oscillator strength --- r_loggf Reference for loggf number=1 References: B92: Bessell M. S. 1992, private communication B,B+,C,C+,D,D-,E: accuracy ratings from NIST (1996) NIST Atomic Spectroscopic Database (Version 1.1) D+92: Davidson et al., 1992A&A...255..457D G+94: Giridhar et al., 1994ApJ...437..476G GS88: Gratton & Sneden, 1988A&A...204..193G H+82: Hannaford et al., 1982ApJ...261..736H K90: Kurucz, 1990, private communication PC89: Peterson & Carney, 1989ApJ...347..266P SC88: Sneden & Crocker, 1988ApJ...335..406S T89: Thevenin, 1989A&AS...77..137T T90: Thevenin, 1990A&AS...82..179T T94: Takeda, 1994PASJ...46...53T WM80: Wiese & Martin, 1980, NSRDS-NBS 60 (U.S. Government Printing Office, Washington, DC) WSM: Wiese, Smith, & Miles, 1969, Atomic Transition Probabilities, Vol 2, NSRDS-NBS 22 (U.S. Government Printing Office, Washington, DC) --- EW(BD+112998) BD+11 2998 Equivalent width 0.1pm u_EW(BD+112998) Uncertainty flag on (BD+112998 --- EW(M2V11) M2_V11 equivalent width 0.1pm u_EW(M2V11) Uncertainty flag on (M2V11) --- EW(M2HII89) M2_HII_89 equivalent width 0.1pm u_EW(M2HII89) Uncertainty flag on (M2HII89) --- EW(M13SH11) M13_SH11 equivalent width 0.1pm u_EW(M13SH11) Uncertainty flag on (M13SH11) --- EW(M13I13) M13_I_13 equivalent width 0.1pm u_EW(M13I13) Uncertainty flag on EW(M13I13) --- EW(M56V6) M56_V6 equivalent width 0.1pm u_EW(M56V6) Uncertainty flag on EW(M56V6) --- EW(M56I60) M56_I_60 equivalent width 0.1pm u_EW(M56I60) Uncertainty flag on EW(M56I60) --- EW(M56I96) M56_I_96 equivalent width 0.1pm u_EW(M56I96) Uncertainty flag on EW(M56I96) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Jun 06 Russell, S. C. [Dublin Institute for Advanced Studies] J_A+A_326_1069.xml Chromospheric models of dwarf M stars J/A+A/326/249 J/A+A/326/249 Chromospheric models of dwarf M stars Chromospheric models of dwarf M stars P Mauas A Falchi L Pasquini R Pallavicini Astron. Astrophys. 326 249 1997 1997A&A...326..249M Models, atmosphere Stars, M-type stars: atmospheres stars: chromospheres stars: late-type Tables 4 and 5 give the atmospheric parameters for our models of dM stars Gl 588 and Gl 628. The columns give the column mass in g/cm^-2^, the electron temperature in K, the microturbulent velocity in km/s; the continuum optical depth at 5000{AA}; the hydrogen, proton, and electron density in particles per cm^-3^; and the height h (in km) above the level where tau_5000_=1.
Gl 588 15 32 18 -41 15 42 Gl 628 16 30 18 -12 38 47
Atmospheric parameters for our model for Gl 588 Atmospheric parameters for our model for Gl 628 Mass Column mass g/cm2 Te Electron temperature K Vtur Microturbulent velocity km/s tau5000 Continuum optical depth at 5000{AA} (500nm) --- NH Hydrogen density cm-3 Np Proton density cm-3 Ne Electron density cm-3 h Height above the level where tau_5000{AA}_=1 km tables.tex TeX version of the tables A. Falchi Osservatorio di Arcetri Patricia Bauer CDS 1997 Apr 10 Ambretta Falchi <falchi@arcetri.astro.it> J_A+A_326_249.xml V, I photometry of the metal-rich bulge globular cluster Terzan 2 J/A+A/326/614 J/A+A/326/614 Terzan 2 VI photometry V, I photometry of the metal-rich bulge globular cluster Terzan 2 S Ortolani E Bica B Barbuy Astron. Astrophys. 326 614 1997 1997A&A...326..614O Clusters, globular Photometry, CCD Galaxy: abundances Galaxy: center globular clusters: individual (Terzan 2) Hertzsprung-Russell (HR diagram) We present for the first time optical colour magnitude diagrams of the globular cluster Terzan 2, in the V, I colours. The horizontal branch is red. The red giant branch morphology can be fitted with that of 47 Tuc, but definitely not th at of NGC 6553. We derive a reddening of E(B-V)=1.54 and a distance d_{sun}_=7.7kpc if R=3.1, or 5.3kpc if R=3.6. Terzan 2 adds to the list of bulge metal-rich clusters now with reliable parameters.
Terzan 2 C 1724-307 17 27 33.1 -30 48 08
V, I photometry of Terzan 2 No sequence number --- Xpos x pixel coordinate in Fig. 1 number=1 North is up and West is to the right pix Ypos y pixel coordinate in Fig. 1 number=1 North is up and West is to the right pix Vmag V magnitudes mag V-I V-I colour index mag Patricia Bauer CDS 1997 Feb 14 Beatriz Barbuy <barbuy@orion.iagusp.usp.br> J_A+A_326_614.xml Ba stars, galactic populations and evolution J/A+A/326/722 J/A+A/326/722 HIPPARCOS Ba stars Ba stars, galactic populations and evolution M -O Mennessier X Luri F Figueras A E Gomez S Grenier J Torra P North Astron. Astrophys. 326 722 1997 1997A&A...326..722M I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) magnitudes, absolute Stars, barium Stars, distances galactic populations kinematics stars: absolute magnitudes stars: Ba stars: evolution HIPPARCOS astrometric and kinematical data together with radial velocities from other sources are used to calibrate both luminosity and kinematics parameters of Ba stars and to classify them. Five distinct classes have been found i.e. some halo stars (H) and four groups belonging to disk population: roughly super-giants (S), two groups of giants (one on the giant branch (G), the other at the clump location(C)) and dwarfs (D). Individual distances and luminosities are estimated.
Hipparcos
Individual estimated parameters HIP HIPPARCOS (Cat. <I/239>) number --- Name HD or BD or CP identifier --- Group Group at which the star has been assigned --- Mvis Absolute visual magnitude mag Dist Distance pc e_Dist Distance error pc var HIPPARCOS variability flag --- dup HIPPARCOS duplicity flag --- Marie-Odile Mennessier GRAAL Patricia Bauer CDS 1997 Sep 04 Marie-Odile Mennessier <menes@graal.univ-montp2.fr> J_A+A_326_722.xml Chemical composition of halo and disk stars with overlapping metallicities J/A+A/326/751 J/A+A/326/751 Chemical composition of halo and disk stars Chemical composition of halo and disk stars with overlapping metallicities P E Nissen W J Schuster Astron. Astrophys. 326 751 1997 1997A&A...326..751N Abundances Photometry, uvby, beta Stars, population II Galaxy: abundances Galaxy: evolution Galaxy: halo stars: abundances stars: Population II Table A1 lists the Stromgren photometry together with color excesses, E(b-y), photometric metallicities, [Fe/H] , calculated from the calibrations of Schuster & Nissen (1989A&A...221...65S), and absolute magnitudes, M(V), and distances derived with the equations of Nissen & Schuster (1991A&A...251..457N) using the photometric metallicities. Table A2 contains coordinates, proper motions and radial velocities for the program stars as well as distances calculated from the calibrations Nissen & Schuster (1991A&A...251..457N) using the spectroscopic metallicities scaled to our photometric [Fe/H] system. Table A3 gives a list of the 209 spectral lines, which were analyzed, arranged element by element. The table contains the wavelength, the excitation potential of the lower level corresponding to the line, the gf-value, the enhancement factor of the classical van der Waals damping constant, the statistical weight of the upper level, and the equivalent widths measured for the two "standard" stars, HD 22879 and HD 76932. Table A4 contains the measured equivalent widths for all program stars. Table A5 gives abundance ratios and kinematical as well as orbital parameters for the program stars. First are given the data for the 16 disk stars, then follows the 14 halo stars.
Stromgren photometry and derived parameters Name Designation of star --- Vmag Visual magnitude number=1 Vmag, b-y, m1 and c1 have been corrected for the effect of interstellar reddening if E(b-y)>0.015. mag b-y Colour index number=1 Vmag, b-y, m1 and c1 have been corrected for the effect of interstellar reddening if E(b-y)>0.015. mag m1 Metallicity index number=1 Vmag, b-y, m1 and c1 have been corrected for the effect of interstellar reddening if E(b-y)>0.015. mag c1 Balmer discontinuity index number=1 Vmag, b-y, m1 and c1 have been corrected for the effect of interstellar reddening if E(b-y)>0.015. mag Hbeta H-beta line index mag E(b-y) Color excess mag [Fe/H] Photometric metallicity [Sun] M(V) Absolute magnitude mag Dist Distance (using photometric metallicities) pc Coordinates, proper motions and radial velocities Name Designation of star --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Epoch Epoch of coordinates --- pmRA Proper motion = 15*mu(alpha)*cos(dec) arcsec/yr pmDE Proper motion = mu(dec) arcsec/yr HRV Heliocentric radial velocity km/s Dist Distance (using spectroscopic metallicities) pc Atomic line data and equivalent widths for the standard stars HD 22879 and HD 76932 Element Chemical element and ionization stage --- Lambda Wavelength (Angstrom) 0.1nm EP Line excitation energy of lower level eV log(gf) Log gf (oscillator strength) --- f6 Enhancement factor of classical van der Waals damping Gamma_6 --- g(upper) Statistical weight of upper level of line --- W(22879) Equivalent width (milliAngstrom) for HD22879 0.1pm W(76932) Equivalent width (milliAngstrom) for HD76932 0.1pm Equivalent widths for the 30 programme stars Element Chemical element and ionization stage --- Lambda Wavelength (Angstrom) 0.1nm EW(1) Equivalent width (mA) for HD3567 0.1pm EW(2) Equivalent width (mA) for CD-61 0282 0.1pm EW(3) Equivalent width (mA) for HD17288 0.1pm EW(4) Equivalent width (mA) for HD17820 0.1pm EW(5) Equivalent width (mA) for G005-040 0.1pm EW(6) Equivalent width (mA) for CD-47 1087 0.1pm EW(7) Equivalent width (mA) for HD22879 0.1pm EW(8) Equivalent width (mA) for HD24339 0.1pm EW(9) Equivalent width (mA) for HD25704 0.1pm EW(10) Equivalent width (mA) for HD241253 0.1pm EW(11) Equivalent width (mA) for G102-020 0.1pm EW(12) Equivalent width (mA) for CD-33 3337 0.1pm EW(13) Equivalent width (mA) for CD-57 1633 0.1pm EW(14) Equivalent width (mA) for CD-45 3283 0.1pm EW(15) Equivalent width (mA) for G088-040 0.1pm EW(16) Equivalent width (mA) for HD76932 0.1pm EW(17) Equivalent width (mA) for G046-031 0.1pm EW(18) Equivalent width (mA) for HD83220 0.1pm EW(19) Equivalent width (mA) for BD-21 3420 0.1pm EW(20) Equivalent width (mA) for HD103723 0.1pm EW(21) Equivalent width (mA) for HD105004 0.1pm EW(22) Equivalent width (mA) for HD106038 0.1pm EW(23) Equivalent width (mA) for HD106516 0.1pm EW(24) Equivalent width (mA) for W7547 0.1pm EW(25) Equivalent width (mA) for HD113083A 0.1pm EW(26) Equivalent width (mA) for HD113083B 0.1pm EW(27) Equivalent width (mA) for HD113679 0.1pm EW(28) Equivalent width (mA) for HD120559 0.1pm EW(29) Equivalent width (mA) for HD121004 0.1pm EW(30) Equivalent width (mA) for HD126681 0.1pm Abundance ratios and kinematical parameters Name Designation of star --- m_Name Multiplicity index on Name --- Teff Effective temperature K log(g) Logarithmic surface gravity [cm/s2] [Fe/H] iron-to-hydrogen ratio --- [O/Fe] Oxygen-to-iron ratio --- [Mg/Fe] Magnesium-to-iron ratio --- [Si/Fe] Silicon-to-iron ratio --- [Ca/Fe] Calcium-to-iron ratio --- [Ti/Fe] Titanium-to-iron ratio --- [Cr/Fe] Chromium-to-iron ratio --- [Ni/Fe] Nickel-to-iron ratio --- [Na/Fe] Sodium-to-iron ratio --- [Y/Fe] Yttrium-to-iron ratio --- [Ba/Fe] Barium-to-iron ratio --- Uvel Galactic U-velocity component relative LSR km/s Vvel Galactic V-velocity component relative LSR km/s Wvel Galactic W-velocity component relative LSR km/s V(tot) Total velocity relative to galactic center km/s H(z) Angular momentum about z-axis of the Galaxy kpc.km/s e Orbital eccentricity --- z(max) Maximum value of z-coordinate kpc R(max) Maximum distance from galactic center kpc z(min) Minimum value of z-coordinate kpc R(min) Minimum distance from galactic center kpc |z|(max) Maximum distance from the galactic plane kpc Patricia Bauer CDS 1997 Aug 25 Poul Erik Nissen <pen@obs.aau.dk> J_A+A_326_751.xml The age-mass relation for chromospherically active binaries. II. Lithium depletion in dwarf components J/A+A/326/780 J/A+A/326/780 Lithium depletion in CABs The age-mass relation for chromospherically active binaries. II. Lithium depletion in dwarf components D Barrado y Navascues M J Fernandez-Figueroa R J Garcia Lopez E De Castro M Cornide Astron. Astrophys. 326 780 1997 1997A&A...326..780B V/76 : Chromospherically Active Binaries (Strassmeier+ 1993) Abundances Photometry, UBVRI Stars, double and multiple binaries: close stars: abundances stars: activity stars: late-type We included 2 tables containing photometric data, together equivalent width of LiI6708 A, for a sample of dwarf components of Chromospherically Active Binaries (CABs).
Photometry and evolutionary classification of the sample of CABs Name Star name --- HD HD Number --- (U-B) (U-B) colour index mag (B-V) (B-V) colour index mag (V-R)j (V-R)j colour index mag (R-I)j (R-I)j colour index mag Dist Distance pc Vmag V magnitude mag Mv V absolute magnitude mag Status Evolutionary status (off, MS) --- SpType Spectral type number=1 Spectral type between brackets are assumed from the photometry --- Com Comments number=2 a: The color indices include the contribution of the secondary, except when the color for the secondary is given. b: Two equal stars: (U-B)_p_=(U-B)_s_=(U-B)_{obs}_, V_p_=V_s_=V_{obs}_+0.753. c: The hot component dominates (U-B). d: There is also available M_V_^p^, M_V_^s^. e: It is possible to deconvolve the photometry in V. f: Combined M_V_. g: The hot component dominates (B-V). h: M_V_(hot/cool) were calculated independently during the eclipses. i: M_V_(primary) were calculated by a deconvolution with the M_V_(total) and M_V_(secondary): V_p_=V_s_ - 2.5log[10^(V_total_-V_s_)/2.5) - 1]. j: M_V_ assumed from the spectral type. k: From the Strassmeier et al. catalogue (Cat. <V/76>). l: Distance from M_V_, V. m: M_V_ from R, T_eff_, CB. --- Equivalent widths and corrections for the observed stars (in mA) Name Star name --- HD HD Number --- Teff Efective temperature K Rad Radius Sun EW(Li+Fe) Li+Fe equivalent width 0.1pm n_EW(Li+Fe) *: Line blended with others --- EW(Fe) Fe equivalent width 0.1pm n_EW(Fe) c: calculated --- EW(Li) Li equivalent width 0.1pm n_EW(Li) c: calculated --- CCF Continuum Correction Factor (c/h) --- Com Comments number=1 1: CCF from Equation 2 and 3 2: CCF from Equation 2 and 4 3: We deconvolved the magnitude of the primary from the total magnitude and an estimation of the magnitude of the secondary by using the spectral type 4: Evolved components --- Final abundances, where and other parameters for CABS Name Star name --- HD HD Number --- Teff Effective temperature K l_EW(Li)c Limit flag on EW(Li)c --- EW(Li)c Corrected Li equivalent width 0.1pm l_N(Li) Limit flag on N(Li) --- N(Li) Li abundance --- l_Mass Limit flag on Mass --- Mass Stellar Mass solMass n_Mass Note on mass number=1 CM: Mass estimated from the color-magnitude diagram Msin3i: Mass computed from M*sin^3^i RT: Mass estimated from Radii-T_eff_ plane --- Porb Orbital Period d l_Pphot Limit flag on Pphot --- Pphot Rotational Period d n_Pphot Note on Pphot number=2 Porb: Photometric period similar to the orbital value --- l_LogAge Limit flag on LogAge --- LogAge Age [yr] n_LogAge Note on LogAge number=3 M: Age estimated from the mass-age relationship. P: Age of the secondary equal to the computed age for the primary --- Age Same age object name (Hyades or V772 Her) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 May 06 David Barrado y Navascues <barrado@mars.harvard.edu> J_A+A_326_780.xml Structure and evolution of low-mass stars J/A+A/327/1039 J/A+A/327/1039 Structure and evolution of low-mass stars Structure and evolution of low-mass stars G Chabrier I Baraffe Astron. Astrophys. 327 1039 1997 1997A&A...327.1039C Abundances Models, evolutionary Stars, masses stars: abundances stars: low-mass, brown dwarfs Properties of Very Low mass stars for different initial metallicity [M/H] and Helium mass fraction: mass (in solar mass), age (in Gyrs) effective temperature (in K), log of luminosity (in solar L), radius (10^10cm), central temperature Tc (in K) and density RHOc (in gr/cm-3). Abundances of light elements are normalised to their initial abundance (see text).
CB97 models ([M/H] = -2 to 0; Y = 0.25 or 0.275) [M/H] Initial metallicity [Sun] Y Initial helium mass fraction --- Mass Mass solMass Age Age Gyr Teff Effective temperature K Lum Luminosity [solLum] Rad Radius 10+8m logTc Central temperature [K] logRHOc Density [g/cm3] Li/Lio Lithium abundance number=1 Abundance normalised to initial abundance --- Be/Beo Berillium abundance number=1 Abundance normalised to initial abundance --- B/Bo Bore abundance number=1 Abundance normalised to initial abundance --- Patricia Bauer CDS 1997 Apr 24 Isabelle Baraffe <Isabelle.Baraffe@ens-lyon.fr> J_A+A_327_1039.xml Long-term photometric flares patrol (1967-1977) on EV Lac: a clear evidence of a longitude concentrated flaring activity in 1970 J/A+A/327/1114 J/A+A/327/1114 Optical flares on EV Lac in 1967-1977 Long-term photometric flares patrol (1967-1977) on EV Lac: a clear evidence of a longitude concentrated flaring activity in 1970 G Leto I Pagano C S Buemi M Rodono Astron. Astrophys. 327 1114 1997 1997A&A...327.1114L Photometry, UBV Stars, flare stars: activity stars: flare stars: individual (EV Lac) stars: rotation We report on a large sample of homogeneous photoelectric data obtained by monitoring the red dwarf flare star EV Lac. The data were collected in 10 years (1967-77) at Catania Astrophysical Observatory on Mt. Etna. The peak luminosity, the total energy emitted, the rise and decay times were measured for each flare.
EV Lac 22 46 52.9 +44 20 25
Summary of flare data No Flare sequential number in year --- OBSdate Observation date "DD/MM/YY" UTmaxh UT flare maximum (hours) h UTmaxm UT flare maximum (minutes) min Band Band --- Tel Telescope diameter cm n_Lmax pl : partially lost (no data following) --- Lmax Luminosity at maximum 10+21W E Integrated flare energy 10+22J Trise Rise-time to the highest peak s Duration Duration of the light decrease to quiescence s Dm Flare amplitude mag e_Dm Error on flare magnitude mag table2.tex LaTeX version of table2 Patricia Bauer CDS 1997 Jun 03 Giuseppe Leto <GLETO@alpha4.ct.astro.it> J_A+A_327_1114.xml Dust around young stars. Photopolarimetric activity of the classical Herbig Ae/Be star RR Tauri. J/A+A/327/145 J/A+A/327/145 Photopolarimetric activity of RR Tauri Dust around young stars. Photopolarimetric activity of the classical Herbig Ae/Be star RR Tauri. A N Rostopchina V P Grinin A Okazaki P S The S Kikuchi D N Shakhovskoy N Kh Minikhulov Astron. Astrophys. 327 145 1997 1997A&A...327..145R Photometry, UBVRI Polarization Stars, variable circumstellar matter polarization stars: individual (RR Tau) stars: pre-main sequence stars: variables: other The results of coordinated Crimea-Dodaira simultaneous multi-bands photometric and polarimetric observations of the classical Herbig Ae/Be star RR Tau which cover fully the observed interval of its brightness changes are presented. Within the observed interval of its light variations the linear polarization of RR Tau anti-correlates with its brightness changes.
RR Tau 05 39 30.5 +26 22 25
RR Tau photometric and polarimetric UBVRI observations at CAO JD Julian date d Vmag V magnitude mag U-B (U-B) color-index mag B-V (B-V) color-index mag V-R (V-R) color-index mag V-I (V-I) color-index mag P(U) Degree of linear polarization in U band % e_P(U) Accuracy of polarization degree in U band % PA(U) Position angle of polarization in U band deg e_PA(U) Accuracy of position angle in U band deg P(B) Degree of linear polarization in B band % e_P(B) Accuracy of polarization degree in B band % PA(B) Position angle of polarization in B band deg e_PA(B) Accuracy of position angle in B band deg P(V) Degree of linear polarization in V band % e_P(V) Accuracy of polarization degree in V band % PA(V) Position angle of polarization in V band deg e_PA(V) Accuracy of position angle in V band deg P(R) Degree of linear polarization in R band % e_P(R) Accuracy of polarization degree in R band % PA(R) Position angle of polarization in R band deg e_PA(R) Accuracy of position angle in R band deg P(I) Degree of linear polarization in I band % e_P(I) Accuracy of polarization degree in I band % PA(I) Position angle of polarization in I band deg e_PA(I) Accuracy of position angle in I band deg The data of RR Tau photometry and polarimetry at Dodaira JD Julian date d V V magnitude mag U-B (U-B) color-index mag u_U-B Uncertainty flag on U-B --- B-V (B-V) color-index mag V-R (V-R) color-index mag Dm2 Magnitude difference on 0.41 {mu}m (Chn2) number=1 The magnitude differences between the comparison and variable stars on 0.41{mu}m (Chn2). mag u_Dm2 Uncertainty flag on Dm2 --- Dm5 Magnitude difference on 0.65 {mu}m (Chn5) number=2 The magnitude differences between the comparison and variable stars on 0.65{mu}m (Chn5). mag Dm7 Magnitude difference on 0.76 {mu}m (Chn7) number=3 The magnitude differences between the comparison and variable stars on 0.76{mu}m (Chn7). mag u_Dm7 Uncertainty flag on Dm7 --- P(U) Degree of linear polarization in U band % e_P(U) Accuracy of polarization degree in U band % PA(U) Position angle of polarization in U band deg e_PA(U) Accuracy of position angle in U band deg P(Chn2) Degree of linear polarization in Chn2 band % e_P(Chn2) Accuracy of polarization degree in Chn2 band % PA(Chn2) Position angle of polarization in Chn2 band deg e_PA(Chn2) Accuracy of position angle in Chn2 band deg P(B) Degree of linear polarization in B band % e_P(B) Accuracy of polarization degree in B band % PA(B) Position angle of polarization in B band deg e_PA(B) Accuracy of position angle in B band deg P(V) Degree of linear polarization in V band % e_P(V) Accuracy of polarization degree in V band % PA(V) Position angle of polarization in V band deg e_PA(V) Accuracy of position angle in V band deg P(Chn5) Degree of linear polarization in Chn5 band % e_P(Chn5) Accuracy of polarization degree in Chn5 band % PA(Chn5) Position angle of polarization in Chn5 band deg e_PA(Chn5) Accuracy of position angle in Chn5 band deg P(R) Degree of linear polarization in R band % e_P(R) Accuracy of polarization degree in R band % PA(R) Position angle of polarization in R band deg e_PA(R) Accuracy of position angle in R band deg P(Chn7) Degree of linear polarization in Chn7 band % e_P(Chn7) Accuracy of polarization degree in Chn7 band % PA(Chn7) Position angle of polarization in Chn7 band deg e_PA(Chn7) Accuracy of position angle in Chn7 band deg Alla Rostopchina Crimean Astrophysical Observatory 1997 May 07 Alla N. Rostopchina <arost@crao.crimea.ua> J_A+A_327_145.xml Spectrophotometric study of southern symbiotic stars J/A+A/327/191 J/A+A/327/191 Spectrophometry of southern symbiotic stars Spectrophotometric study of southern symbiotic stars J Mikolajewska A Acker B Stenholm Astron. Astrophys. 327 191 1997 1997A&A...327..191M III/174 : Atlas of line profiles of symbiotic stars (VanWinckel+, 1994) Reddening Spectrophotometry Stars, double and multiple binaries: symbiotic circumstellar matter Hertzsprung-Russell (HR diagram) stars: fundamental parameters We have analyzed the optical spectra of 67 symbiotic stars and objects suspected of being symbiotic, and found 18 new symbiotic systems. This is the largest homogeneous set of optical spectrophotometric data for symbiotic binaries ever studied. We have derived the reddenings and distances for all systems, estimated the IR classes (S and D) for the new systems, and determined the location of the hot components in the Hertzsprung-Russell diagram.
Emission line fluxes in units of 10^-13^erg/cm^2^/s Star Star name ---- HJD Heliocentric Julian date d S6563 6563{AA} emission line flux 10-16W/m2 S4860 HI 4860{AA} emission line flux 10-16W/m2 S4310 HI 4310{AA} emission line flux 10-16W/m2 u_S4310 Uncertainty flag on S4310 --- S4100 4100{AA} emission line flux 10-16W/m2 S4363 4363{AA} emission line flux 10-16W/m2 u_S4363 Uncertainty flag on S4363 --- S4960 [OIII] 4960{AA} emission line flux 10-16W/m2 S5007 5007{AA} emission line flux 10-16W/m2 u_S5007 Uncertainty flag on S5007 --- S5876 5876{AA} emission line flux 10-16W/m2 u_S5876 Uncertainty flag on S5876 --- S6678 HeI 6678{AA} emission line flux 10-16W/m2 u_S6678 Uncertainty flag on S6678 --- S7065 7065{AA} emission line flux 10-16W/m2 u_S7065 Uncertainty flag on S7065 --- S4886 HeII 4886{AA} emission line flux 10-16W/m2 u_S4886 Uncertainty flag on S4886 --- S5412 HeII 5412{AA} emission line flux 10-16W/m2 u_S5412 Uncertainty flag on S5412 --- S6825 OVI 6825{AA} emission line flux 10-16W/m2 u_S6825 Uncertainty flag on S6825 --- S5721 [FeVII] 5721{AA} emission line flux 10-16W/m2 u_S5721 Uncertainty flag on S5721 --- S6086 [FeVII] 6086{AA} emission line flux 10-16W/m2 Reddening estimates Star Star name --- Type Type (S: stellar; D: dusty) --- E(B-V)HIb Reddening from HI (case B) data mag E(B-V)HI Reddening from H I data, lower limit if n_E(B-V)HI = '/' mag n_E(B-V)HI / : interval of reddening --- E(B-V)HIu Upper reddening value from H I data mag l_tauHa Limit flag on TauHa --- tauHa Optical depth in H{alpha} --- n_tauHa / : interval of optical depth --- tauHau Upper limit in Optical depth when interval --- E(B-V)HeI Reddening from He I data mag u_E(B-V)HeI Uncertainty flag on E(B-V)HeI --- E(B-V)HeII Reddening from He II data mag u_E(B-V)HeII Uncertainty flag on E(B-V)HeII --- E(B-V)Fe Reddening from [Fe VII] data mag u_E(B-V)Fe Uncertainty flag on E(B-V)Fe --- E(B-V)IR Reddening from Ir data mag u_E(B-V)IR Uncertainty flag on E(B-V)IR --- E(B-V) Adopted reddening mag Physical parameters Star Star name --- Type Type (S: stellar; D: dusty) --- SpType1 Spectral type from this study --- SpType2 Spectral type from other references --- l_Dist Limit flag on Dist --- Dist Distance kpc u_Dist Uncertainty flag on Dist --- Ion Ion --- Th Temperature or lower limit if n_Th='/' 10+3K n_Th / : interval of temperature --- Thu Upper limit of temperature when interval 10+3K l_Lh Limit flag on Lh --- Lh Luminosity solLum tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Sep 23 Joanna Mikolajewska <Joanna_Mikolajewska@camk.edu.pl> J_A+A_327_191.xml The molecular gas content of spiral galaxies in the Coma/A1367 supercluster J/A+A/327/522 J/A+A/327/522 Molecular gas content of spiral galaxies The molecular gas content of spiral galaxies in the Coma/A1367 supercluster A Boselli G Gavazzi J Lequeux V Buat F Casoli J Dickey J Donas Astron. Astrophys. 327 522 1997 1997A&A...327..522B Galaxies, spectra Radio lines galaxies: general galaxies: spiral intergalactic medium ISM: general radio lines: galaxies stars: formation We present 12CO(J=1-0) line observations of 73 spiral galaxies mostly in the Coma/A1367 supercluster. From these data, combined with data available in the literature, we extract the first complete, optically selected sample (mpg<15.2) of 37 isolated and of 27 cluster galaxies. The 12CO(1-0) line spectra are accessible as postscript figures.
Target galaxies CGCG CGCG designation number=1 The first 3 digits indicate the field number, the last 3 the source number in the field; see catalog <VII/49>. --- NGC/IC NGC/IC number --- UGC Designation in UGC <VII/26> --- RAh Right Ascension B1950 (hours) number=2 Celestial coordinates with a few arcsec accuracy, from Gavazzi & Boselli (1996), Astrophys. Letters and Comm. 35, 1 h RAm Right Ascension B1950 (minutes) number=2 Celestial coordinates with a few arcsec accuracy, from Gavazzi & Boselli (1996), Astrophys. Letters and Comm. 35, 1 min RAs Right Ascension B1950 (seconds) number=2 Celestial coordinates with a few arcsec accuracy, from Gavazzi & Boselli (1996), Astrophys. Letters and Comm. 35, 1 s DE- Declination B1950 (sign) number=2 Celestial coordinates with a few arcsec accuracy, from Gavazzi & Boselli (1996), Astrophys. Letters and Comm. 35, 1 --- DEd Declination B1950 (degrees) number=2 Celestial coordinates with a few arcsec accuracy, from Gavazzi & Boselli (1996), Astrophys. Letters and Comm. 35, 1 deg DEm Declination B1950 (minutes) number=2 Celestial coordinates with a few arcsec accuracy, from Gavazzi & Boselli (1996), Astrophys. Letters and Comm. 35, 1 arcmin DEs Declination B1950 (seconds) number=2 Celestial coordinates with a few arcsec accuracy, from Gavazzi & Boselli (1996), Astrophys. Letters and Comm. 35, 1 arcsec MType Morphological type from Gavazzi+Boselli (1996) --- Agg Aggregation (membership) note number=3 The Aggregation note has the following values: A = member of A1367 C = member of Coma cluster I = isolated; G = group; P = pair; N = NGC 5056 group I, G, P and N are all included in the Coma supercluster region (see Gavazzi, 1987ApJ...320...96G for more details) H51 and H97 = member of A2151 and A2197 in the Hercules supercluster, cA and cD = member of the cloud A and D in the Cancer cluster (Bothun et al. 1984AJ.....89.1300B). --- RVel Heliocentric velocity, from Gavazzi (1989ApJ...346...59G) and references therein. km/s Distance Distance determined using Ho = 100km/s/Mpc number=4 we assume 69 Mpc for the Coma cluster and 65 Mpc for A1367 as in Gavazzi (1987ApJ...320...96G) For galaxies belonging to groups, the distances are determined from their average redshifts. For double systems or isolated supercluster objects, distances are determined from the individual redshifts. Cloud A Cancer galaxies are taken at 47 Mpc, cloud D at 36 Mpc. Galaxies in the Hercules supercluster are assumed at 110 Mpc (A2151), and at 92 Mpc (A2197). Mpc MajDiam Galaxy major diameter number=5 Galaxy major and minor optical blue diameters, in arcminutes, from Gavazzi & Boselli (1996). These are isophotal diameters at the 25th mag/arcsec2 determined from available CCDs. arcmin MinDiam Galaxy minor diameter number=5 Galaxy major and minor optical blue diameters, in arcminutes, from Gavazzi & Boselli (1996). These are isophotal diameters at the 25th mag/arcsec2 determined from available CCDs. arcmin Pmag Photographic magnitude as given in the CGCG. mag HIwidth Width of the HI line number=6 Width of the HI line averaged between 20 and 50 % of its maximum, from Gavazzi (1989ApJ...346...59G) and references therein. km/s Results of CO observations CGCG CGCG designation, as in table1.dat --- Itime Integration time (on+off) min rms rms noise, in mK, in the T*R scale. mK l_I(CO) Limit flag on I(CO) --- I(CO) Intensity of the I(CO) line number=1 For undetected galaxies, the reported value is an upper limit determined as follows: I(CO) = 2{sigma} ({Delta}V(HI).{delta}V(CO))^1/2^ where {sigma} is the rms noise of the spectrum, {Delta}V(HI) is the HI line width {delta}V(CO) is the spectral resolution = 20 km/s For galaxies with {Delta}V(HI) not available, the HI width has been determined assuming a standard {Delta}V(HI) = 300 sin(i) km/s, where i is the galaxy inclination, or {Delta}V(HI) = 50 km/s if i = 0. K.km/s e_I(CO) Error on CO intensity I(CO) number=2 The error e_I(CO) is computed as e_I(CO) = 2{sigma} ({Delta}V(CO).{delta}V(CO))^1/2^ where {sigma} is the rms noise of the spectrum, {Delta}V(CO) is the CO linewidth (given in Col. 7), and {delta}V(CO) is the spectral resolution. Spectra were smoothed to {delta}V(CO) = 20 km/s K.km/s V(CO) Heliocentric velocity from the CO line number=3 Heliocentric velocity determined with a gaussian fit (optical definition v=cz={Delta}{lambda}/{lambda}_0_). The estimated error is comparable with the resolution, thus 20 km/s km/s DV(CO) Width at 50% of the CO line km/s l_logMiH2 Limit flag on logMiH2 --- logMiH2 "Indicative" H_2_ mass (see Sect. 4.1) [solMass] File File name (in subdirectory fig) number=4 two figures are missing because the FITS files were corrupted. --- Parameters of the optically selected galaxies CGCG CGCG designation number=1 The first 3 digits indicate the field number, the last 3 the source number in the field; see catalog <VII/49>. --- MType Morphological type from Gavazzi+Boselli (1996) --- Agg Membership note number=2 as in Table 1, the Aggregation note has the following values: A = member of A1367; C = member of Coma cluster; I = isolated; G = group; P = pair; N = NGC 5056 group --- W05 Cluster membership assigned number=3 Cluster membership assigned according to the statistical method described in Gavazzi et al. (1995ApJ...438..590G), based on dynamical considerations (hereafter referred as the "caustic" criterium). If W is the weighting function defined in Gavazzi et al. 1995 for {Omega}o = 0.5, indicating the probability to a galaxy to reside within the caustic (thus the probability to be dynamically related to the cluster), we assume cluster members those objects with W > 0.80 and isolated galaxies those with W < 0.80. As discussed in Gavazzi et al., the "caustic" criterium is less restrictive than the "aggregation" criterium since it includes in the cluster sample some objects at larger angular distances. --- MajDiam Galaxy major diameter as in table1.dat arcmin MinDiam Galaxy minor diameter as in table1.dat arcmin Distance determined using H0 = 100 km/s/Mpc Mpc Hc Corrected H magnitude from Gavazzi+Boselli (1996) mag Bc Corrected B magnitude from Gavazzi+Boselli (1996) mag UV Uncorrected UV 200nm magnitude number=4 From Donas et al. (1990A&A...235...60D; 1995A&A...303..661D) mag l_M(HI) Limit flag on M(HI) --- M(HI) logarithm of the atomic hydrogen mass, as in Gavazzi (1987ApJ...320...96G) [solMass] l_HIdef Limit flag on HIdef --- HIdef HI deficiency, determined as in Haynes and Giovanelli (1984AJ.....89..758H) --- l_MiH2 Limit flag on MiH2 --- MiH2 Logarithm of the indicative molecular hydrogen content, as described in section 4.1. [solMass] Ref References to the CO data number=5 References are: 1) this work, 1994 run; 2) this work, 1995 run; 3) this work, 1996 run; 4) Boselli et al. (1994A&A...285...69B); 5) Boselli et al. (1995A&AS..110..521B); 6) Casoli et al. (1991A&A...249..359C); 7) Dickey & Kazes (1992ApJ...393..530D); 8) Casoli et al. (1996A&AS..116..193C) --- r Ratio of optical diameter to HPBW number=6 ratio r of the optical diameter to the HPBW of the telescope used in the CO observations. The note indicates: m indicates mapped objects; galaxies marked * indicates the galaxies observed also with the 12m Kitt Peak telescope (HPBW = 55"; see Casoli et al. 1996A&AS..116..193C), with consistent results. r gives a raw estimate of the CO sampling of the target galaxy. Given the peaked CO distribution compared with the optical one (see Sect. 4.1), the observations should give accurate measurement of the total CO emission of galaxies with r<2, while they should underestimate by a factor of <2 the total CO emission of objects with r=4 (Sauty et al., in preparation). --- n_r Note on r number=6 ratio r of the optical diameter to the HPBW of the telescope used in the CO observations. The note indicates: m indicates mapped objects; galaxies marked * indicates the galaxies observed also with the 12m Kitt Peak telescope (HPBW = 55"; see Casoli et al. 1996A&AS..116..193C), with consistent results. r gives a raw estimate of the CO sampling of the target galaxy. Given the peaked CO distribution compared with the optical one (see Sect. 4.1), the observations should give accurate measurement of the total CO emission of galaxies with r<2, while they should underestimate by a factor of <2 the total CO emission of objects with r=4 (Sauty et al., in preparation). --- Halpha Halpha equivalent width from Gavazzi et al. (1991AJ....101.1207G) + references therein. 0.1nm n_Halpha Recently observed galaxy number=7 An * indicates galaxies recently observed, for which only preliminary data (used in the following analysis) are available; these H{alpha} data will be presented in a forecoming paper (Gavazzi et al., in preparation). --- U-B (U-B)c Corrected colour from Gavazzi+Boselli (1996) mag l_FIR/H Limit flag on FIR/H --- FIR/H Far IR to U ratio in logarithmic scale number=8 the ratio FIR/H, in logarithmic scale, determined from the 60um FIR flux (in mJy) and the Hflux (in mJy), defined as Hflux = 1.030x10^6^ . 10^-Hc/2.5^ mJy. [] Patricia Bauer CDS 1997 Jun 09 Alessandro Boselli <BOSELLI@astrsp-mrs.fr> J_A+A_327_522.xml The rise and fall of the NaMgAl stars J/A+A/327/587 J/A+A/327/587 Abundances of 9 solar-type stars The rise and fall of the NaMgAl stars J Tomkin B Edvardsson D L Lambert B Gustafsson Astron. Astrophys. 327 587 1997 1997A&A...327..587T Abundances, peculiar Equivalent widths Stars, dwarfs Galaxy: abundances Galaxy: evolution stars: abundances stars: fundamental parameters Line identifications, measured equivalent widths and derived chemical abundances in 9 solar-type dwarf stars, which are identified by their Bright Star (HR, (Cat. <V/50>)) numbers.
HR 448 HD 9562 01 33 42.2 -07 01 27 HR 1536 HD 30562 04 48 35.3 -05 40 14 HR 3176 HD 67228 08 07 45.7 +21 34 58 HR 3951 HD 86728 10 01 02.7 +31 55 47 HR 4027 HD 88986 10 16 28.3 +28 41 01 HR 4688 HD 107213 12 19 30.3 +28 09 31 HR 8041 HD 199960 21 00 33.6 -04 43 42 HR 8472 HD 210855 22 11 47.1 +56 50 15 HR 8729 HD 217014 22 57 27.1 +20 46 04
Stellar equivalent widths and abundances HR HR (Cat. <V/50>) number --- Element Chemical element, e.g. 'N ' or 'Fe' --- Ion 'I ': neutral atom, 'II': singly ionized atom --- Wavel Rest frame line wavelength (Angstrom) 0.1nm EW Measured equivalent width (milliA) number=1 Blank fields when no equivalent widths were measured and no abundance was derived 0.1pm Abund Derived element abundance (1) number=2 The abundances are logarithmic element abundances [X/H] relative to the Sun, see footnote 1 of the main reference [Sun] Bengt Edvardsson Uppsala Astron. Obs. Patricia Bauer CDS 1997 Sep 04 Bengt Edvardsson <be@astro.uu.se> J_A+A_327_587.xml Otical-IUE observations of the gamma-loud BL Lacertae object S5 0716+714: data and interpretation J/A+A/327/61 J/A+A/327/61 BV Otical-IUE observations of the gamma-loud BL Lacertae object S5 0716+714: data and interpretation G Ghisellini M Villata C M Raiteri S Bosio G De Francesco G Latini M Maesano E Massaro F Montagni R Nesci G Tosti M Fiorucci E Pian L Maraschi A Treves A Comastri M Mignoli Astron. Astrophys. 327 61 1997 1997A&A...327...61G BL Lac objects Photometry, Cousins Photometry, UBVRI BL Lacertae objects: general BL Lacertae objects: individual (S5 0716+714) gamma-rays: theory ultraviolet: galaxies Table 2 reports the journal of observations. For each date the measured magnitudes and their uncertainties in the four filters together with the used telescope are given. In some occasions several images were made in the course of the same night to search for intraday variability; these nights are indicated by an asterisk. The magnitude uncertainties have been evaluated by taking into account the mean dispersion of the internal error, but not the errors on the absolute calibration.
S5 0716+714 QSO 0716+714 07 21 53.4 +71 20 36
Observed magnitudes of S5 0716+714 Date Observation date "DD/MM/YY" n_Date Note on observations number=1 The asterisk indicates the nights in which more than four observations with the same telescope were performed. --- HJD Heliocentric JUlian day d Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag Rcmag R_c magnitude mag e_Rcmag rms uncertainty on Rcmag mag Icmag I_c magnitude mag e_Icmag rms uncertainty on Icmag mag Tel Telescope number=2 Telescope identifications: R = Roma , P = Perugia, T = Torino --- table2.tex LaTeX version of table2 Ghisellini Osserv. di Brera Patricia Bauer CDS 1997 Jun 26 Gabriele Ghisellini <gabriele@merate.mi.astro.it> J_A+A_327_61.xml On the mass distribution of planetary nebulae central stars J/A+A/327/736 J/A+A/327/736 Planetary nebulae properties On the mass distribution of planetary nebulae central stars G Stasinska S K Gorny R Tylenda Astron. Astrophys. 327 736 1997 1997A&A...327..736S J/A+A/303/893 : Planetary nebulae with WR-type nuclei (Gorny+, 1995) J/A+A/318/256 : Planetary nebulae properties (Gorny+ 1997) J/A+A/299/755 : Stellar evolution. II. Post-AGB (Bloecker+, 1995) Abundances Morphology Planetary nebulae planetary nebulae: general stars: AGB and post-AGB stars: fundamental parameters white dwarfs We apply a method, described in Gorny et al. (1997, Cat. <J/A+A/318/256>), to derive the masses of 125 central stars of planetary nebulae (PN). This method is self-consistent and distance-independent. It requires the knowledge of the nebular H{beta} fluxes, angular radii and expansion velocities, as well as the stellar visual magnitudes. This method is based on a simple model for the evolution of planetary nebulae, in which the central stars evolve according to the theoretical models of Bloecker (1995, Cat. <J/A+A/299/755>) and Schoenberner (1983ApJ...272..708S). The results are dependent on the assumed total nebular mass. Nevertheless, for any reasonable total nebular mass distribution, we find that the range in planetary nebulae central star masses is very restricted: more than 80% of the objects have a central star mass between 0.55 and 0.65M_{sun}_. We show how to convert, in this mass range, the observed PN central star mass distribution into a zero-age post-AGB star mass distribution.
Planetary nebulae properties and derived central stars masses, evolutionary ages and distances PNG PNG (Cat. <V/84>) designation --- Name Name --- Mtype Morphological type number=1 Morphological type description: e,E,EH: elliptical nebulae B,BE: bipolar nebulae P,PE: point symmetric nebulae I: irregular nebulae --- u_Mtype Uncertainty flag on morphological type --- log(THI) logarithm of HI Zanstra temperature [K] log(LHI) logarithm of HI Zanstra luminosity [solLum] Mv Central star absolute visual magnitude mag log(Rad) logarithm of nebular radius [pc] log(SuBr) logarithm of nebular surface brightness in H{beta} [mW/m2/sr] log(Sv) logarithm of S_v parameter [mW/m2/sr] DistS Shklovsky distance kpc l_Mass Lower limit flag on central star's mass --- Mass Derived mass of the central star solMass MassUp Upper limit to the central star's mass (where existing, one case only) solMass Age Derived evolutionary age 10+3yr Dist Derived distance kpc Patricia Bauer CDS 1997 Aug 01 Slawomir K. Gorny <skg@ncac.torun.pl> J_A+A_327_736.xml Search for H_2_O maser emission from high-latitude IRAS sources J/A+A/327/755 J/A+A/327/755 OH maser emission from IRAS sources Search for H_2_O maser emission from high-latitude IRAS sources F Palla C Codella R Valdettaro C Baffa Astron. Astrophys. 327 755 1997 1997A&A...327..755P J/A+A/277/453 : OH maser survey of cool IRAS sources (David+ 1993) Infrared sources Masers Radio lines galaxies: starburst ISM: clouds masers stars: formation A high-sensitivity search for water maser emission at 22.2 GHz has been performed on a sample of 91 IRAS point sources at high-latitudes. The aim of the survey is to verify if these clouds are capable of star formation as indicated by the presence of water masers. The sample is based on the recent work of Magnani et al. (1995ApJS...96..159M) who have identified 192 infrared objects from the IRAS Faint Source Survey possibly associated with translucent clouds at galactic latitudes |b|>=30{deg}. These IRAS sources have far-infrared colours typical of young stellar objects and pre-main-sequence stars and thus provide a starting list for further studies about their actual nature. H_2_O maser emission is a good diagnostic of the presence of dense gas and of recent star formation. We did not find water maser emission at a level of 0.2-0.5Jy (3{sigma}) in any of the 91 objects. The negative result indicates that these high-latitude sources do not represent potential sites of star formation, consistent with the fact that most high-latitude molecular clouds do not appear gravitationally bound.
IRAS
</tableLink> </tableLinks> <fields> <field> <name>Name</name> <definition>Source Name</definition> <units>---</units> </field> <field> <name>IRAS</name> <definition>IRAS Source Name</definition> <units>---</units> </field> <field> <name>RAh</name> <definition>Right Ascension (1950)</definition> <units>h</units> </field> <field> <name>RAm</name> <definition>Right Ascension (1950)</definition> <units>min</units> </field> <field> <name>RAs</name> <definition>Right Ascension (1950)</definition> <units>s</units> </field> <field> <name>DE-</name> <definition>Declination sign</definition> <units>---</units> </field> <field> <name>DEd</name> <definition>Declination (1950)</definition> <units>deg</units> </field> <field> <name>DEm</name> <definition>Declination (1950)</definition> <units>arcmin</units> </field> <field> <name>DEs</name> <definition>Declination (1950)</definition> <units>arcsec</units> </field> <field> <name>rms</name> <definition>Noise of the spectrum</definition> <units>Jy</units> </field> </fields> </tableHead> <history> <ingest> <creator> <lastName>Patricia Bauer</lastName> <affiliation>CDS</affiliation> </creator> <date> <year>1997</year> <month>Jul</month> <day>09</day> </date> <acknowledgement>Claudio Codella <codella@oan.es></acknowledgement> </ingest> </history> <identifier>J_A+A_327_755.xml</identifier> </dataset> <dataset subject="astronomy" xmlns:xlink="http://www.w3.org/XML/XLink/0.9"> <title>Velocity structure of the dwarf galaxy population in the Centaurus cluster J/A+A/327/952 J/A+A/327/952 Centaurus cluster velocities Velocity structure of the dwarf galaxy population in the Centaurus cluster P Stein H Jerjen M Federspiel Astron. Astrophys. 327 952 1997 1997A&A...327..952S J/A+AS/124/1 : The Centaurus Cluster Catalogue (Jerjen+ 1997) Clusters, galaxy Radial velocities galaxies: clusters: general galaxies: distances and redshifts galaxies: evolution galaxies: individual (Centarus cluster, NGC 4696) Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen & Dressler, 1997, Cat. <J/A+AS/124/1>) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&S0, spirals, Im&BCD, and dE&dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.
New redshifts for Centaurus cluster members New redshifts of background galaxies Reobserved redshifts for Centaurus cluster members Seq Sequential number --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec CCC Centaurus Cluster Catalogue (Jerjen & Dressler 1996, Cat. <J/A+AS/124/1>) reference number --- Mtype Morphological type --- BT Total blue magnitude mag SBeff Effective surface brightness mag/arcsec+2 Prob Cen 45 cluster member probability number=1 If prob=0.00, this automatically implies that the galaxy is a 100% Cen 30 member. % Vcc Cross-correlation redshift km/s e_Vcc rms uncertainty on Vcc km/s Vem Emission line redshift km/s e_Vem rms uncertainty on Vem km/s cz Heliocentric radial velocity number=2 Weighted average of Vccf and Vemi. km/s e_cz rms uncertainty on cz km/s table5.tex LaTeX version of table5 table5.ps PostScript version of table5 Patricia Bauer CDS 1998 Jan 26 Martin Federspiel <martin@astro.unibas.ch> J_A+A_327_952.xml No stellar age gradient inside supergiant shell LMC4. J/A+A/328/167 J/A+A/328/167 BV photometry in supergiant shell LMC4 No stellar age gradient inside supergiant shell LMC4. J M Braun D J Bomans J -M Will K S De Boer Astron. Astrophys. 328 167 1997 1997A&A...328..167B I/221 : The Magellanic Catalogue of Stars - MACS (Tucholke+ 1996) ftp://ftp.astro.uni-bonn.de/pub/jbraun/p1_lmc4 : Magellanic Clouds Photometry, CCD Photometry, UBV Hertzsprung-Russell (HR diagram) ISM: bubbles ISM: individual (LMC 4) Magellanic Clouds stars: early-type stars: luminosity function, mass function The file table1.dat shows the entire photometry. It consists of 25 CCD fields, each taken at the ESO 0.91 m Dutch telescope in April, 1993. With 10min B and 5min V exposures it reaches down to V = 20-21mag (depending on seeing). The table structure is that of the published Table 1 plus additional information about right ascension and declination. Thus the announced Table 3 had been omitted (note that the entire MACS catalogue is also available electronically, as Cat. <I/221>). The file fig3.ps is a finding chart of the CCD fields made from four (i.e. 44, 45, 51, 52) mosaiced V charts of the LMC atlas of Hodge & Wright (1967, "The Large Magellanic Cloud", Smithsonian Press). This chart is a version of Fig. 3 with better quality (i.e. new labels, slightly larger view etc.) and additionally marked fields C1, C2, and C3 of a new (January 1999) B, V photometry which will soon be available (see the authors homepage). The youngest stellar populations of a 'J'-shaped region inside the supergiant shell (SGS) LMC4 have been analysed with CCD photometry in B, V passbands. This region consists of 2 coherent strips, one from the east to the west reaching about 400pc across the OB superassociation LH 77 and another extending about 850pc from south to north. The standard photometric methods yield for each of the 25 CCD fields a colour-magnitude diagram (CMD) which is used for age determination of the youngest star population by isochrone fitting. The resultant ages lie in the range from 9Myr to 16Myr without correlation with the distance to the LMC 4 centre. We therefore conclude that there must have been one triggering event for star formation inside this large LMC SGS with a diameter of 1.4kpc.
Photometry of the 'J' area inside LMC 4 FieldSeq Field Sequence Field Sequence is a floating point derived by field number (0-24) plus star sequence number (at most 4 digits) divided by 10000. The fields are marked in Fig. 3 included as fig3.ps. regions (Nos a-e) and fields (Nos 0-24) not in SIMBAD --- xtotal X coordinate of total area pix ytotal Y coordinate of total area pix xfield X coordinate of respective CCD field pix yfield Y coordinate of respective CCD field pix Vmag V magnitude mag e_Vmag Total error in Vmag Total errors including systematic and statistic errors (see paper). mag B-V B-V colour mag e_B-V Total error in B-V mag MV0 Absolute (intrinsic) V magnitude mag (B-V)0 Intrinsic B-V colour mag RAh Right Ascension J2000 (hours) The given coordinates are derived by cross identification with MACS stars. The mean derivation from the reference grid is 0.27s, 1.1" respectively. h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec fig3.ps Mosaic chart of the LMC4 area with the positions Jochen M. Braun Stw., Univ. Bonn Patricia Bauer CDS 1999 Aug 10 Jochen M. Braun <jbraun@astro.uni-bonn.de> J_A+A_328_167.xml High resolution infrared spectroscopy of CN and NH lines: nitrogen abundance in oxygen-rich giants through K to late M J/A+A/328/175 J/A+A/328/175 K & M giants equivalent widths High resolution infrared spectroscopy of CN and NH lines: nitrogen abundance in oxygen-rich giants through K to late M W Aoki T Tsuji Astron. Astrophys. 328 175 1997 1997A&A...328..175A Equivalent widths Spectra, infrared Stars, giant stars: abundances stars: AGB and post-AGB stars: atmospheres stars: late-type The analyses of high resolution infrared spectra have been done for CN lines in oxygen-rich cool evolved stars including 2 K giants, 20 M giants and 1 S-type star. Since CN lines analyzed in the present work are weak and resolved well, they are appropriate for quantitative analyses. CN lines of {DELTA}v=-2 and -1 sequences (red system) which are in the K- and the H-window regions, respectively, give the consistent nitrogen abundance for each star. The analyses of NH lines in the L-window region have been done for 5 late M giants for which CN lines have been also analyzed. Although the triplet structure of NH lines cannot be fully resolved, they are preferable because determination of nitrogen abundance is almost independent of other elemental abundances while nitrogen abundance based on CN depends on carbon abundance. The nitrogen abundances derived from NH for late M giants agree well with those from CN for which we adopt 7.75eV as the dissociation energy in the analysis. The results show that the nitrogen abundances in late M giants are larger than those in early M giants while decrease of the carbon abundance was found in late M giants by our previous work (Tsuji, 1991A&A...245..203T). These variations of abundances can not be explained by the first dredge-up model but require additional processing by the CN cycle and mixing after the first dredge-up. However, there is no obvious evidence of other processes such as the 3{alpha}-process and subsequent hot bottom burning in our program stars. Such variation of the carbon and nitrogen abundances is not well understood by the present evolutionary models of low-mass and intermediate-mass stars.
CN lines in K- and H-windows region in K and early M giants CN lines in K- and H-windows region in late M giants Name Star name --- Window Window --- Line Line --- WN Wavenumber cm-1 log(gf) log of oscillation strength --- LEP Lower excitation potential cm-1 log(EW) Equivalent width [0.1nm] NH lines in L-window region in late M type giants Name Star name ---- Line Line ---- WN Wavenumber cm-1 LEP Lower excitation potential cm-1 log(gf)1 log of oscillation strength number=1 The equivalent widths are measured for two or three components of the triplet structure together with the 3 gf values given. --- log(gf)2 log of oscillation strength number=1 The equivalent widths are measured for two or three components of the triplet structure together with the 3 gf values given. --- log(gf)3 log of oscillation strength number=1 The equivalent widths are measured for two or three components of the triplet structure together with the 3 gf values given. --- log(EW) Equivalent width [0.1nm] Patricia Bauer CDS 1997 Sep 22 Wako Aoki <waoki@mtk.ioa.s.u-tokyo.ac.jp> J_A+A_328_175.xml Spectroscopic analysis of the Alpha Centauri System J/A+A/328/261 J/A+A/328/261 Spectroscopy of Alpha Cen Spectroscopic analysis of the Alpha Centauri System C Neuforge-Verheecke P Magain Astron. Astrophys. 328 261 1997 1997A&A...328..261N Abundances Stars, double and multiple binaries: visual stars: abundances stars: fundamental parameters stars: individual (alpha Cen) This table presents the results of a spectroscopic analysis (differentially to the Sun) of the two components of the binary system Alpha Centauri. This analysis has been carried out on the basis of extensive high resolution and high signal-to-noise spectra taken at the European Southern Observatory (La Silla, Chile).
alpha Cen A HR 5459 HD 128620 14 40 00.8 -60 50 42 alpha Cen B HR 5460 HD 128621 14 40 00.7 -60 50 38
Spectroscopic data and abundances in Alpha Cen A, Alpha Cen B and the Sun. Elm Element and ionisation stage --- AbundSun Solar abundance (1) number=2 For the CN molecule, the solar abundance indicated is that of N. --- lambda Wavelength of the line 0.1nm EP Excitation potential of the lower level eV log(gf) Solar oscillator strength in log10 --- EWsc Solar equivalent width at the disk center 0.1pm EWs Solar equivalent width in integrated light 0.1pm AbundSun2 Solar abundance from EW in integrated light --- EWa Equivalent width in Alpha Cen A 0.1pm AbundA Abundance in Alpha Cen A number=1 The abundance of an element is given on the usual logarithmic scale relative to hydrogen: A(el)=(log(Nel/NH) + 12) Nel and NH being respectively the number densities of the element and of hydrogen. --- EWb Equivalent width in Alpha Cen B 0.1pm AbundB Abundance in Alpha Cen B number=1 The abundance of an element is given on the usual logarithmic scale relative to hydrogen: A(el)=(log(Nel/NH) + 12) Nel and NH being respectively the number densities of the element and of hydrogen. --- Patricia Bauer CDS 1997 Aug 25 Corinne Neuforge <Corinne.Neuforge@ulg.ac.be> J_A+A_328_261.xml The role of convection on the uvby colours of A, F, and G stars J/A+A/328/349 J/A+A/328/349 Role of Convection in A, F, and G stars The role of convection on the uvby colours of A, F, and G stars B Smalley F Kupka Astron. Astrophys. 328 349 1997 1997A&A...328..349S Abundances Models, atmosphere Photometry, uvby convection stars: atmospheres stars: fundamental parameters stars: general stars: late-type We discuss the effects of convection on the theoretical uvby colours of A, F, and G stars. The standard mixing-length theory atlas9 models of Kurucz (1993, ATLAS9, SAO, Cambridge, USA), with and without approximate overshooting, are compared to models using the turbulent convection theory proposed by Canuto & Mazzitelli (1991ApJ...370..295C, 1992ApJ...389..724C) and implemented by Kupka (1996, ASPConf. Proc. 108, 73). Comparison with fundamental Teff and log g stars reveals that the Canuto & Mazzitelli models give results that are generally superior to standard mixing-length theory (MLT) without convective overshooting. MLT models with overshooting are found to be clearly discrepant. This is supported by comparisons of non-fundamental stars, with Teff obtained from the Infrared Flux Method and log g from stellar evolutionary models for open cluster stars. The Canuto & Mazzitelli theory gives values of (b-y)0 and c0 that are in best overall agreement with observations. Investigations of the m0 index reveal that all of the treatments of convection presented here give values that are significantly discrepant for models with Teff<6000K. It is unclear as to whether this is due to problems with the treatment of convection, missing opacity, or some other reason. None of the models give totally satisfactory m0 indices for hotter stars, but the Canuto & Mazzitelli models are in closest overall agreement above 7000K. Grids of uvby colours, based on the CM treatment of convection, are presented. These grids represent an improvement over the colours obtained from models using the mixing-length theory. The agreement with fundamental stars enables the colours to be used directly without the need for semi-empirical adjustments that were necessary with the earlier colour grids. For a description of the uvby photometric system, see e.g. <GCPD/04>
*Canuto & Mazzitelli (CM) grid for [M/H] = +1.0 CM grid for [M/H] = +0.5 CM grid for [M/H] = +0.0 CM grid for [M/H] = -0.5 </tableLink> </tableLinks> <fields> <field> <name>Teff</name> <definition>Teff</definition> <units>K</units> </field> <field> <name>log(g)</name> <definition>log g</definition> <units>[cm/s2]</units> </field> <field> <name>[M/H]</name> <definition>Metallicity [M/H]</definition> <units>[Sun]</units> </field> <field> <name>Vturb</name> <definition>microturbulence</definition> <units>km/s</units> </field> <field> <name>u-b</name> <definition>u-b colour index</definition> <units>mag</units> </field> <field> <name>b-y</name> <definition>b-y colour index</definition> <units>mag</units> </field> <field> <name>m1</name> <definition>m1 colour index</definition> <units>mag</units> </field> <field> <name>c1</name> <definition>c1 colour index</definition> <units>mag</units> </field> </fields> </tableHead> <tableHead> <tableLinks> <tableLink xlink:href="table5"> <title>Comparison between evolutionary and grid log g HD HD (Cat. <III/135>) number --- Teff Teff from Kunzli et al. (1997, Cat. <J/A+AS/122/51>) K logg logg from evolutionary models (Kunzli et al., 1997, Cat. <J/A+AS/122/51>) [cm/s2] b-y b-y colour index mag c0 c0 colour index mag Teff(CM) Teff from CM (Canuto & Mazzitelli) grid number=1 Canuto & Mazzitelli models, 1991ApJ...370..295C and 1992ApJ...389..724C. K logg(CM) logg from CM grid [cm/s2] Dlogg(CM) Delta logg for CM grid [cm/s2] Teff(noOV) Teff from MLT (mixing-length theory) noOV grid K logg(noOV) logg from MLT noOV grid [cm/s2] Dlogg(noOV) Delta logg for MLTnoOV grid [cm/s2] Teff(OV) Teff from MLT OV grid K logg(OV) logg from MLT OV grid [cm/s2] Dlogg(OV) Delta logg for MLT OV grid [cm/s2] Patricia Bauer CDS 1997 Jul 30 Barry Smalley <bs@astro.keele.ac.uk> J_A+A_328_349.xml Properties and nature of Be stars. XVIII. Spectral, light and colour variations of 4 Herculis J/A+A/328/551 J/A+A/328/551 Spectroscopic data of 4 Herculis Properties and nature of Be stars. XVIII. Spectral, light and colour variations of 4 Herculis P Koubsky P Harmanec J Kubat A -M Hubert H Bozic M Floquet P Hadrava G Hill J R Percy Astron. Astrophys. 328 551 1997 1997A&A...328..551K J/A+A/324/965 : UBV photometry of V360 Lac. Paper 17. (Hill+ 1997) Harmanec et al., (88 Her) Paper 1. 1972BAICz..23..218H Harmanec et al., (88 Her) Paper 2. 1972ApL....11..119H Harmanec et al., (4 Her) Paper 3. 1973A&A....22..337H Harmanec et al., (88 Her) Paper 4. 1974A&A....33..117H Heard et al., (4 Her) Paper 5. 1975A&A....42...47H Harmanec et al., (4 Her) Paper 6. 1976BAICz..27...47H Doazan et al., (88 Her) Paper 7A. 1982A&AS...50..481D Doazan et al., (88 Her) Paper 7B. 1982A&A...115..138D Harmanec et al., (88 Her) Paper 8. 1978BAICz..29..278H Koubsky, (HD 174237) Paper 9. 1978BAICz..29..288K Koubsky et al., (CX Dra) Paper 10. 1980BAICz..31...75K Horn et al., (HD 184279) Paper 11. 1982BAICz..33..308H Stefl, (KX And) Paper 12. 1985BAICz..36..313S Koubsky et al., (HD 183656) Paper 13. 1989BAICz..40...31K Stefl et al., (KX And) Paper 14. 1990BAICz..41...29S Harmanec et al., (LQ And) Paper 15. 1991BAICz..42....1H Juza et al., (5 kappa Dra) Paper 16. 1991BAICz..42...39J Binaries, spectroscopic Radial velocities Stars, Be binaries: spectroscopic stars: emission-line, Be stars: individual (4 Her) stars: variables: general A collection of spectroscopic data of 4 Her at our disposal (RV and spectrophotometric measurements) consist of spectra obtained at the Ondrejov and Haute Provence Observatories. Table 1 summarizes the measurements of radial velocities and line intensities carried out in the red spectra. In Table 2 a list of the spectra and RV measurements for the violet-blue region is given.
HD 142926 4 Her HR 5938 15 55 30.6 +42 33 57
H{alpha} data No Plate or file number number=1 no letter - Ondrejov photographic spectra r - Reticon a - Aurelie --- Disp Dispersion 0.1nm/mm HJD Heliocentric Julian day d RVem Radial velocity of the H-alpha emission wings km/s RVshell Radial velocity of the H-alpha shell line km/s V/R Ratio of the violet to red peak of the Halpha emission --- V Relative intensity of the violet peak of the H-alpha emission --- R Relative intensity of the red peak of the H-alpha emission --- Ic Relative central intensity of H-alpha --- RVSiII Radial velocity of the SiII 6347A line km/s RVabs Radial velocity of the absorption feature in the H-alpha emission km/s Radial velocities on blue spectrograms No Plate or file number number=1 no letter - Ondrejov photographic spectra W - OHP 1.93 GB - OHP 1.52 a - Aurelie --- Disp Dispersion 0.1nm/mm HJD Heliocentric Julian day d shell Indication of a shell number=2 N - no shell, blank - shell --- RVH Mean radial velocity of broad hydrogen lines km/s w_RVH Weight of RVH number=3 see Eq.1 in a paper --- RVHshell Radial velocity of hydrogen shell lines km/s w_RVHshell Weight of RVHshell number=3 see Eq.1 in a paper --- RVHe Mean radial velocity of helium lines km/s w_RVHe Weight of RVHe number=3 see Eq.1 in a paper --- RVMshell Mean radial velocity of metallic shell lines km/s Patricia Bauer CDS 1997 Aug 25 Jiri Kubat <kubat@sunstel.asu.cas.cz> J_A+A_328_551.xml Chemistry and rotational excitation of O2 in interstellar clouds. II - The ^16^O^18^O isotopomer J/A+A/328/617 J/A+A/328/617 16^O 18^O isotopomer collision rate Chemistry and rotational excitation of O2 in interstellar clouds. II - The ^16^O^18^O isotopomer P Marechal Y P Viala L Pagani Astron. Astrophys. 328 617 1997 1997A&A...328..617M Atomic physics Radio lines ISM: abundances ISM: molecules molecular processes radio lines: ISM In this paper, a chemical model of interstellar clouds including ^18^O and ^13^C isotopic reactions with a non-LTE calculations of ^16^O^18^O rotational population has been used to predict the intensity of the three ^16^O^18^O lines observable from the ground, namely 234, 298 and 402GHz.
Collision rates ^16^O^18^O-He (cm^3/s) Collision rates ^16^O^18^O-He (cm^3/s) Collision rates ^16^O^18^O-He (cm^3/s) Nu N value of the upper level --- Ju J value of the upper level --- Nl N value of the lower level --- Jl J value of the lower level --- a0 Collision rate factor (k_ul_=a_0-*T^0.3^) --- table4.tex LaTeX version of table4 Patricia Bauer CDS 1997 Jun 12 Priscilla MARECHAL <priscila@mesiom.obspm.fr> J_A+A_328_617.xml Determination of the globular cluster and halo stellar mass functions and stellar and brown dwarf densities J/A+A/328/83 J/A+A/328/83 Globular clusters luminosity function Determination of the globular cluster and halo stellar mass functions and stellar and brown dwarf densities G Chabrier D Mera Astron. Astrophys. 328 83 1997 1997A&A...328...83C Clusters, globular Magnitudes Stars, M-type dark matter Galaxy: stellar content stars: low-mass, brown dwarfs stars: luminosity function, mass function Data of figure 1 of the paper, namely the luminosity function of globular clusters in bolometric magnitude. The original HST magnitude is given, then the corresponding bolometric magnitude and the converted luminosity function. The vertical scale of the LF is arbitrary (it is the scale used on the figure). The conversion between the HST and bolometric magnitudes uses a spline fit of the theoretical models of Baraffe et al. (1997A&A...327.1054B), for the appropriate metallicities. The name of the cluster and of the observational paper main authors are given as a header, followed by the magnitudes description and the data.
Bolometric luminosity function Name Globular cluster name --- Ref References to the observational paper number=1 MP : De Marchi and Paresce (1995A&A...304..211D) S : Santiago et al. (1996MNRAS.281.1363S) FP : Fusi-Pecci et al. (1996, preprint) E : Elson et al. (1995AJ....110..682E) P : Paresce et al. (1995ApJ...442L..57P) C : Cool et al. (1996ApJ...468..655C) M : Mould (1996PASP..108..682M) --- n_mag HST magnitude band (I814, V555 or V606) --- mag Magnitude in band specified by n_mag mag Mbol Bolometric magnitude mag log(FL) Luminosity function (stellar density as a function of bolometric magnitude) in log scale --- Patricia Bauer CDS 1997 Oct 14 Dominique Mera <dmera@cral.ens-lyon.fr> J_A+A_328_83.xml Investigation of the Pleiades cluster. IV. The radial structure. J/A+A/329/101 J/A+A/329/101 Masses of Pleiades members Investigation of the Pleiades cluster. IV. The radial structure. D Raboud J -C Mermilliod Astron. Astrophys. 329 101 1998 1998A&A...329..101R J/A+A/320/74 : Radial velocities of Pleiades members (Mermilliod+ 1997) Rosvick et al., Paper I. 1992A&A...255..130R Mermilliod et al., Paper II. 1992A&A...265..513M Mermilliod et al., Paper III. 1997A&A...320...74M = Cat. <J/A+A/320/74> Clusters, open Stars, masses binaries: spectroscopic open clusters and associations: individual (Pleiades) On the basis of the best available member list and duplicity information, we have studied the radial distribution of 270 stars and multiple systems earlier than K0 in the Pleiades. Five new long period spectroscopic binaries have been identified from the CORAVEL observations. We have found a clear mass segregation between binaries and single stars, which is explained by the greater average mass of the multiple systems. The mass function of the single stars and primaries appears to be significantly different. While the central part of the cluster is spherical, the outer part is clearly elliptical, with an ellipticity of 0.17. The various parameters describing the Pleiades are (for a distance of 125pc): core radius r_c_=0.6 deg (1.4pc), tidal radius r_t_=7.4 (16pc), half mass radius r_m/2_=0.88 (1.9pc), harmonic radius r=1.82 (4pc). Low-mass stars (later than K0) probably extend further out and new proper motion and radial velocity surveys over a larger area and to fainter magnitudes would be very important to improve the description of the cluster structure and complete mass function.
Pleiades Cl Melotte 22 03 47.0 +24 07
Star member list in the Pleiades HII Star number from Herzsprung (See Cat. <I/90>) --- Vmag V magnitude mag B-V B-V colour mag xpos x coordinate number=1 x is oriented West to East (- --> +) y is oriented South to North (- -> +) arcmin ypos y coordinate number=1 x is oriented West to East (- --> +) y is oriented South to North (- -> +) arcmin Dist Distance from the cluster center arcmin Mult Multiplicity status --- Rem Remarks --- Mass Total mass solMass MassA Component A mass solMass MassB Component B mass solMass MassC Component C mass solMass MassD Component D mass solMass Patricia Bauer CDS 1997 Aug 20 Didier Raboud <Didier.Raboud@obs.unige.ch> J_A+A_329_101.xml Simultaneous observations of maser lines of ^28^SiO in evolved stars J/A+A/329/219 J/A+A/329/219 28SiO in O-rich evolved stars Simultaneous observations of maser lines of ^28^SiO in evolved stars J R Pardo J Cernicharo E Gonzalez-Alfonso V Bujarrabal Astron. Astrophys. 329 219 1998 1998A&A...329..219P Masers Radio lines Stars, O circumstellar matter masers radio lines: stars stars: AGB and post-AGB We present simultaneous observations of several rotational lines of ^28^SiO in the v=1, 2, 3, and 4 vibrationally excited states toward O-rich evolved stars. All the data were taken in a relatively short period of 65 days, which allows a comparative study of the ^28^SiO maser lines intensities and profiles. The observed differences concerning intensity and line shape among the different maser lines suggest that infrared overlaps deeply affect the pumping of some SiO masers. We qualitatively discuss this effect with consideration to the IR overlaps at 8 {mu}m between the various SiO isotopomers and between ^28^SiO and water vapor
IRC +10011 WX Psc 01 06 25.9 +12 35 53 S Per HD 14528 02 22 51.7 +58 35 12 IK Tau 03 53 28.5 +11 24 20 TX Cam 05 00 54 +56 11 18 IRC+ 50137 NV Aur 05 11 19.4 +52 52 34 R Leo HD 84748 HR 3882 09 47 33.4 +11 25 46 R Aql HD 177940 HR 7243 19 06 22.1 +08 13 51 RR Aql HD 188915 19 57 36.2 -01 53 11 NML Cyg V1489 Cyg 20 46 25.6 +40 06 56 T Cep HD 202012 HR 8113 21 09 32.2 +68 29 28 mu Cep HD 206936 HR 8316 21 43 30.3 +58 46 48 R Cas HD 224490 HR 9066 23 58 24.3 +51 23 18
Parameters of detected ^28^SiO lines Star Star name --- Line Line identification (quantum numbers) --- VPeak Peak velocity km/s HWPeak Peak halfwidth km/s IntArea Integrated area Jy.km/s tab5-16.ps Post-Script version of tab5-16 Patricia Bauer CDS 1997 Dec 15 Juan Pardo <pardo@khamsin.giss.nasa.gov> J_A+A_329_219.xml SMART97: a new solution for the rotation of the rigid Earth J/A+A/329/329 J/A+A/329/329 SMART97, rigid Earth rotation new solution SMART97: a new solution for the rotation of the rigid Earth P Bretagnon G Francou P Rocher J L Simon Astron. Astrophys. 329 329 1998 1998A&A...329..329B VI/63 : Earth Orbit, Precession and Insolation -20Myr to +10Myr (Laskar+ 1993) J/A+A/312/1017 : Coefficients of rigid Earth nutation. I. (Souchay+, 1996) J/AJ/110/1420 : Nutation of the Earth (Williams 1995) Earth Positional data astrometry celestial mechanics, stellar dynamics Earth The Earth rotation solution SMART97 (Solution du Mouvement de l'Axe de Rotation de la Terre) is an analytical solution of the Earth rotation in the rigid case. It gives the expressions of precession-nutation and rotation of the Earth for the 3 Euler angles {psi}, {omega}, {phi} as well as for the quantities p, {epsilon}, {chi}, and the sidereal time. For the axis of figure (fig), these 7 quantities are given in the dynamical system (dyn) and in the kinematical system (kin). SMART97 also gives the variables {psi} and {omega}, in the dynamical system, for the differences (axis of figure - axis of rotation) (rot) and (axis of figure - axis of the angular momentum) (ang). The accuracy of the solution is better than 2.2 microarcseconds for all these variables over 20000 days, between 1968 and 2023. A program EXAMPLE (Fortran 77) is provided which makes use of the subroutine SMART97 which substitutes the time in the series of the solutions SMART97.
(axis of figure - axis of rotation) in the dynamical reference system, variable {psi} (axis of figure - axis of rotation) in the dynamical reference system, variable {omega} (axis of figure - axis of the angular momentum) in the dynamical reference system, variable {psi} (axis of figure - axis of the angular momentum) in the dynamical reference system, variable {omega} axis of figure in the kinematical reference system, variable {psi} axis of figure in the kinematical reference system, variable {omega} axis of figure in the kinematical reference system, variable {phi} axis of figure in the kinematical reference system, variable p axis of figure in the kinematical reference system, variable {epsilon} axis of figure in the kinematical reference system, variable {chi} axis of figure in the kinematical reference system, variable sidereal time axis of figure in the dynamical reference system, variable {psi} axis of figure in the dynamical reference system, variable {omega} axis of figure in the dynamical reference system, variable {phi} axis of figure in the dynamical reference system, variable p axis of figure in the dynamical reference system, variable {epsilon} axis of figure in the dynamical reference system, variable {chi} axis of figure in the dynamical reference system, variable sidereal time ia code of the axis number=1 The codes of the axis are : ia = 1 for the axis of figure 2 for (axis of figure - axis of rotation) 3 for (axis of figure - axis of the angular momentum) --- ib code of the system number=2 The codes of the system are : ib = 1 for the dynamical reference frame 2 for the kinematical reference frame --- ic code of the variable number=3 The codes of the variable are : ic = 1 for psi 2 for omega 3 for phi 4 for p 5 for epsilon 6 for chi 7 for the sidereal time --- k degree k of time variable t --- n rank of the term in a series --- r1 coefficient r of argument --- r2 coefficient r of argument --- r3 coefficient r of argument --- r4 coefficient r of argument --- r5 coefficient r of argument --- r6 coefficient r of argument --- r7 coefficient r of argument --- r8 coefficient r of argument --- r9 coefficient r of argument --- r10 coefficient r of argument --- r11 coefficient r of argument --- r12 coefficient r of argument --- S amplitude S (in microarcseconds/[(100yr)^k^]) --- K amplitude C (in microarcseconds/[(100yr)^k^)]) --- A amplitude a --- B phase b rad C frequency c (in rad/100yr) 10-2rad/yr smart97.doc Notice for use of SMART97 files figdyn97.psi axis of figure in the dynamical reference system, variable {psi} figkin97.psi axis of figure in the kinematical reference system, variable {psi} rotdyn97.psi (axis of figure - axis of rotation) in the dynamical reference system, variable {psi} angdyn97.psi (axis of figure - axis of the angular momentum) in the dynamical reference system, variable {psi} Patricia Bauer CDS 1998 Mar 23 Pierre Bretagnon <pierre@bdl.fr> J_A+A_329_329.xml uvby photometry of theta Coronae Borealis during 1994 and 1995 J/A+A/329/579 J/A+A/329/579 uvby photometry of theta CrB uvby photometry of theta Coronae Borealis during 1994 and 1995 J Fabregat S J Adelman Astron. Astrophys. 329 579 1998 1998A&A...329..579F Photometry, uvby Stars, Be stars: emission-line, Be stars: individual (theta CrB) We present differential uvby photometry of {theta} CrB obtained in 1994 and 1995, complemented by Balmer line spectroscopy. This star has been constant during this period, showing no short term periodic variability with an amplitude greater than 0.005mag., nor long term variations greater than 0.01mag. The lack of variability is associated with an inactive phase of the Be star, in which no emission features are present in the spectra. The only remarkable event observed was a fading episode on JD 2449779, with an amplitude of about 0.02 magnitudes in all bandpasses and duration of 0.2-0.3 days.
theta CrB HD 138749 HR 5778 15 32 55.8 +31 21 33
CAM photometry, v-c data CAM photometry, c-ch data HJD Julian date d Dymag Differential magnitude, y filter mag Dbmag Differential magnitude, b filter mag Dvmag Differential magnitude, v filter mag Dumag Differential magnitude, u filter mag FCAPT photometry, all data HJDu Julian date for the u filter data d Du(v-c) v-c differential magnitude, u filter mag Du(v-ch) v-ch differential magnitude, u filter mag Du(c-ch) c-ch differential magnitude, u filter mag HJDv Julian date for the v filter data d Dv(v-c) v-c differential magnitude, v filter mag Dv(v-ch) v-ch differential magnitude, v filter mag Dv(c-ch) c-ch differential magnitude, v filter mag HJDb Julian date for the b filter data d Db(v-c) v-c differential magnitude, b filter mag Db(v-ch) v-ch differential magnitude, b filter mag Db(c-ch) c-ch differential magnitude, b filter mag HJDy Julian date for the y filter data d Dy(v-c) v-c differential magnitude, y filter mag Dy(v-ch) v-ch differential magnitude, y filter mag Dy(c-ch) c-ch differential magnitude, y filter mag Patricia Bauer CDS 1997 Dec 02 Juan Fabregat <juan@pleione.matapl.uv.es> J_A+A_329_579.xml Sensitivity indicators of Fraunhofer lines J/A+A/329/721 J/A+A/329/721 Sensitivity indicators of Fraunhofer lines Sensitivity indicators of Fraunhofer lines V A Sheminova Astron. Astrophys. 329 721 1998 1998A&A...329..721S Stars, atmospheres Sun Sun: atmosphere Sun: photosphere The results of calculations of the sensitivity indicators to the temperature, as well as the average geometrical heights of localization of the effective response to the temperature variations are presented for the central line depths, for the line depths on half-width, and for the equivalent widths of the 604 Fe I and 58 Fe II absorption lines. This list of unblended solar lines in the range of the wavelengths 401.0-901.0nm contains the maximum of lines suitable for the analysis of the fine structure of the line profiles and primarily for study of the line asymmetries.
The Fe I lines The Fe II lines lambda Wavelength nm EP Lower-level excitation potential eV log(gf) Calculated oscillator strength --- Robs Observed central line depth --- EWcal Calculated equivalent width pm H(R) Heights (central line depths) km H(0.5R) Heights (line depths on half-widths) km H(EW) Heights (equivalent widths) km I(R) Indicators (central line depths) --- I(0.5R) Indicators (line depths on half-widths) --- I(EW) Indicators (equivalent widths) --- Sheminova Main Astronomical Observatory of Ukrainian NAS 1997 May 07 Valentina A. Sheminova <shem@mao.kiev.ua> J_A+A_329_721.xml Revised ages for stars in the solar neighbourhood J/A+A/329/943 J/A+A/329/943 F & G solar neighbourhood stars new ages Revised ages for stars in the solar neighbourhood Y K Ng G Bertelli Astron. Astrophys. 329 943 1998 1998A&A...329..943N J/A+A/275/101 : Chemical evolution of the galactic disk I. (Edvardsson+ 1993) Stars, ages Stars, masses Stars, nearby Hertzsprung-Russell (HR diagram) methods: data analysis solar neighborhood stars: general New ages are computed for the stars from the Edvardsson et al. (1993, Cat. <J/A+A/275/101>) data set. The revised values are systematically larger toward older ages (t>4Gyr), while they are slightly lower for t<4Gyr. A similar, but considerably smaller trend is present when the ages are computed with the distances based on Hipparcos parallaxes. The resulting age-metallicity relation has a small, but distinct slope of ~0.07dex/Gyr.
*F & G stars on or near the main sequence data (no corrections for absolute visual magnitude) *F & G stars on or near the sub-giant branch data (no corrections for absolute visual magnitude) *F & G stars on or near the main sequence data (correction for absolute visual magnitude) *F & G stars on or near the sub-giant branch data (correction for absolute visual magnitude) *F & G stars on or near the main sequence data (as in table3 but with Hipparcos parallax) *F & G stars on or near the sub-giant branch data (as in table4 but with Hipparcos parallax) Cat HR (Cat. <V/50>) or HD (Cat. <III/135>) --- No Star ID number --- Mass Average mass in M_{Sun}_ solMass e_Mass Estimated uncertainty in the mass solMass log(Age) Average age [Gyr] e_log(Age) Estimated uncertainty in log(age) [Gyr] Fit Number of good fits out of the possible 7 from which the average values are obtained. See Note number=1 Special meaning for Fit values: 0: no good fit was obtained at all and the average values and their associated uncertainties are obtained from the `second' best values 1: then only 1 good value was obtained. The average values refer to the good fit only, while the estimated uncertainties are obtained from the 1-good and 6-`second' best values --- log(Age)2 age obtained from a visual inspection of an isochrone through each point (in table4 only) [Gyr] Patricia Bauer CDS 1997 Nov 10 Yuen Keong Ng <yuen@astrpd.pd.astro.it> J_A+A_329_943.xml Broad band energy distribution of ROSAT detected quasars. II. Radio-quiet objects J/A+A/330/108 J/A+A/330/108 ROSAT detected quasars. II. Broad band energy distribution of ROSAT detected quasars. II. Radio-quiet objects W Yuan W Brinkmann J Siebert W Voges Astron. Astrophys. 330 108 1998 1998A&A...330..108Y VII/188 : Quasars and Active Galactic Nuclei (7th Ed.) (Veron+ 1996) IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) IX/11 : ROSAT Source Catalog (Voges+ 1994) J/A+A/319/413 : ROSAT detected quasars. I. (Brinkmann+ 1997) QSOs X-ray sources galaxies: active quasars: general X-rays: galaxies We have compiled a sample of all radio-quiet quasars or quasars without radio detection from the Veron-Cetty - Veron catalogue (1993, VV93, Cat. <VII/166>) detected by ROSAT in the ALL-SKY SURVEY (RASS, Voges 1992, in Proc. of the ISY Conference `Space Science', ESA ISY-3, ESA Publications, p.9, See Cat. <IX/10>), as targets of pointed observations, or as serendipitous sources from pointed observations publicly available from the ROSAT point source catalogue (ROSAT-SRC, Voges et al. 1995, Cat. <IX/11>). For all sources we used the results of the Standard Analysis Software System (SASS, Voges et al. 1992, in Proc. of the ISY Conference `Space Science', ESA ISY-3, ESA Publications, p.223), employing the most recent processing for the Survey data (RASS-II, Voges et al. 1996, Cat. <IX/10>). The total number of quasars is 846. 69 of the radio-quiet objects with radio detections have already been presented in a previous paper (Brinkmann, Yuan, & Siebert 1997, Cat. <J/A+A/319/413>) using the RASS-I results. 17 objects were found to be radio-loud from recent radio surveys and were marked in the table. When available, the power law photon indices and the corresponding absorption column densities (NH) were estimated from the two hardness ratios given by the SASS, both with free fitted NH and for Galactic absorption. The unabsorbed X-ray flux densities in the ROSAT band (0.1-2.4keV) were calculated from the count rates using the energy to counts conversion factor for power law spectra and Galactic absorption. As the photon index we used the value obtained for the individual source if the estimated 1-{sigma} error is smaller than 0.5, otherwise we used the redshift-dependent mean value (see the paper for details).
ROSAT
ROSAT detected radio-quiet quasars IAU IAU name of the object --- n_IAU A flag for classification *: object selected in other wave bands (X-ray, etc.) than in optical %: object found to be radio-loud in recent radio surveys (PMN, NVSS) ?: identification of the X-ray source is uncertain (see text) !: the X-ray flux might be contaminated by a nearby source --- VV93 Alternative name from VV93 (Cat. <VII/166>) --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (Sign or blank) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (') arcmin DEs Declination J2000 (") arcsec z Redshift A '0' as the 3rd decimal is mostly an artifact of the machine readable form of the catalogue. See the printed version of VV93 (Cat. VII/166>) for the appropriate values. --- Vmag Magnitude from VV93 (Cat. <VII/166>) See the printed version of VV93 (Cat. VII/166>) for the appropriate values. mag FX Unabsorbed X-ray flux density (0.1-2.4keV) 10-12mW/m2 e_FX Error of X-ray flux density : One {sigma} statistical errors from count rates only 10-12mW/m2 Gfree X-ray photon index (free fitted NH) Spectral photon index in the ROSAT energy band for a power law fit (S=C*E**(-Gamma)) with free fitted absorption --- E_Gfree Positive error of photon index Gfree One {sigma} errors. If no error is given, the value of the error is unphysically large. --- e_Gfree Negative error of photon index Gfree --- NH X-ray absorbing column density 10+20cm-2 E_NH Positive error of column density 10+20cm-2 e_NH Negative error of column density 10+20cm-2 Ggal X-ray photon index (Galactic absorption) Spectral photon index in the ROSAT energy band for a power law fit (S=C*E**(-Gamma)) with fixed Galactic absorption --- E_Ggal Positive error of photon index Ggal --- e_Ggal Negative error of photon index Ggal --- NHgal Galactic column density Galactic column density from Dickey & Lockman (1990ARA&A..28..215D), see the paper. 10+20cm-2 Com Notes on the X-ray detection S: detected in RASS; P: detected in pointed observations --- Ref Reference for the quoted spectral index BJ: Bechtold J. et al., 1994AJ....108..374B LA: Laor A. et al., 1997ApJ...477...93L RD: Reimers D. et al., 1995A&A...296L..49R SN: Schartel N. et al., 1996, Cat. <J/A+A/307/33> UM: Ulrich M. et al., 1996ApJ...457...77U VC: Vignali C. et al., 1997MmSAI..68..141V WT: Wang T. et al., 1996, Cat. <J/A+A/309/81> --- Patricia Bauer CDS 1997 Dec 16 Weimin Yuan <wey@rzg.mpg.de> J_A+A_330_108.xml Circumstellar emission from dust envelopes around carbon stars showing the silicon carbide feature J/A+A/330/505 J/A+A/330/505 Carbon stars IR emission Circumstellar emission from dust envelopes around carbon stars showing the silicon carbide feature A Blanco A Borghesi S Fonti V Orofino Astron. Astrophys. 330 505 1998 1998A&A...330..505B II/198 : Vilnius photometry of carbon stars (Paupers+, 1993) III/156 : Cool Galactic Carbon Stars, 2nd Edition (Stephenson 1989) Infrared sources Stars, carbon circumstellar matter infrared: stars stars: carbon Spectroscopic and photometric data relative to a sample of 55 carbon stars showing the 11.3{mu}m feature have been fitted in the wavelength range between 0.4 and 100{mu}m by means of a radiative transfer model using the laboratory extinction spectra of amorphous carbon and silicon carbide (SiC) grains. The transfer code allows to determine in a self-consistent way the grain equilibrium temperature of the various species at different distances from the central star and gives all the relevant circumstellar parameters which can be very important for the evolutionary study of carbon stars. In order to get meaningful information on the nature and physical properties of the dust grains responsible for the 11.3{mu}m feature and the underlying continuum, the fitting procedure of the spectr a has been applied individually to every single source. For this reason it has been possible to take into account any variation in position and shape of the band from source to source. Our analysis show that all the sources, in addition to the amorphous carbon grains accounting for the continuum emission, need always the presence of {alpha}-SiC particles while some of them require also {beta}-SiC. Moreover, the presence of one or both types of SiC particles seems not correlated neither with the total optical thickness nor with any other physical and geometrical parameters of the circumstellar envelope. The best-fit parameters found in this work have been used to calculate the mass-loss rate from the central stars. The clear correlation, that we find between the strength of the SiC feature and the total mass loss-rate, confirms the results already found by other authors for the same kind of sources and derived from the observed CO emission lines.
The carbon star sample IRAS IRAS name --- Name Name from Yamashita (1972AnTok..13..169Y, 1975AnTok..15...47Y) --- SpType Spectral type from Yamashita (1972AnTok..13..169Y, 1975AnTok..15...47Y) --- IRC IRC identification (Neugebauer & Leighton 1969IRC...C......0N) --- RAFGL RAFGL identification (Price & Murdock 1983AFGL..161.....P) --- CS Number in the General Catalogue of Cool Carbon Stars (Stephenson 1989, Cat. <III/156>) --- 3um Presence and intensity of the band at 3{mu}m number=1 a - weak b - intermediate c - strong --- 8.6um Presence and intensity of the band at 8.6{mu}m number=1 a - weak b - intermediate c - strong --- 14um Presence and intensity of the band at 14{mu}m number=1 a - weak b - intermediate c - strong --- Best-fit model parameters of our IRAS source sample and computed mass-loss rates IRAS IRAS name --- tau Optical thickness --- T* Stellar temperature K RI/R* Enveloppe inner radius versus stellar radius --- RE/RI Enveloppe outer radius versus stellar radius --- AC AC submicronic grains percentage % alpha {alpha}-SiC submicronic grains percentage % beta {beta}-SiC submicronic grains percentage % dM/dt Computed mass-loss rate solMass/yr tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Dec 18 J_A+A_330_505.xml The absolute magnitudes of RR Lyrae from HIPPARCOS parallaxes and proper motions J/A+A/330/515 J/A+A/330/515 RR Lyrae parallaxes & proper motions The absolute magnitudes of RR Lyrae from HIPPARCOS parallaxes and proper motions J Fernley T G Barnes I Skillen S L Hawley C J Hanley D W Evans E Solano R Garrido Astron. Astrophys. 330 515 1998 1998A&A...330..515F III/176 : RR Lyrae Metallicities (Layden 1994) VI/45 : A bibliographical catalogue of RR Lyrae stars (Heck 1988) Abundances, [Fe/H] Parallaxes, trigonometric Proper motions Radial velocities Stars, variable globular clusters: general Magellanic Clouds RR Lyrae variable We have used HIPPARCOS proper motions and the method of Statistical Parallax to estimate the absolute magnitude of RR Lyrae stars. In addition we used the HIPPARCOS parallax of RR Lyrae itself to determine it's absolute magnitude. These two results are in excellent agreement with each other and give a zero-point for the RR Lyrae M_v_,[Fe/H] relation of 0.77+/-0.15 at [Fe/H]=-1.53. This zero-point is in good agreement with that obtained recently by several groups using Baade-Wesselink methods which, averaged over the results from the different groups, gives M_v_=0.73+/-0.14 at [Fe/H]=-1.53. Taking the HIPPARCOS based zero-point and a value of 0.18+/-0.03 for the slope of the M_v_,[Fe/H] relation from the literature we find firstly, the distance modulus of the LMC is 18.26+/-0.15 and secondly, the mean age of the Globular Clusters is 17.4+/-3.0 GYrs. These values are compared with recent estimates based on other "standard candles" that have also been calibrated with HIPPARCOS data. It is clear that, in addition to astrophysical problems, there are also problems in the application of HIPPARCOS data that are not yet fully understood.
Basic data Star Star name --- n_Star c for RRc, else RRab number=1 The identification of the 'c' types is from the Fourier components as discussed in section 2.3 --- Per Period number=2 Periods were initially from the GCVS (Kholopov et al. 1985, Cat. <II/139>)) and then refined using the HIPPARCOS photometry as discussed in section 2.1 d plx Trigonometric parallax number=3 Trigonometric Parallaxes and proper motions (and their errors) are from HIPPARCOS mas e_plx rms uncertainty on plx mas pmRA Proper motion in RA, {mu}_{alpha}_cos{delta} number=3 Trigonometric Parallaxes and proper motions (and their errors) are from HIPPARCOS mas/yr e_pmRA rms uncertainty on pmRA mas/yr pmDE Proper motion in DE, {mu}_{delta}_ number=3 Trigonometric Parallaxes and proper motions (and their errors) are from HIPPARCOS mas/yr e_pmDE rms uncertainty on pmDE mas/yr Vmag V_J_ magnitude number=4 V_J_ magnitudes are intensity mean magnitudes derived from the HIPPARCOS photometry using the procedures described in section 2.1. The error on these mean magnitudes is typically +/-0.02 mag Kmag K magnitude number=5 K magnitudes are from (1) the Baade-Wesselink analyses listed in Skillen et al. (1993MNRAS.265..301S) (2) Fernley, Skillen and Burki (1993A&AS...97..815F) (3) Unpublished. Typically these have uncertainties of +/-0.04 mag r_Kmag Reference for K magnitudes number=5 K magnitudes are from (1) the Baade-Wesselink analyses listed in Skillen et al. (1993MNRAS.265..301S) (2) Fernley, Skillen and Burki (1993A&AS...97..815F) (3) Unpublished. Typically these have uncertainties of +/-0.04 --- E(B-V) Reddening number=6 E(B-V) is from (1) Burstein and Heiles (1982AJ.....87.1165B) (2) Using the Log(P)-(V-K) relations discussed in Section 2.2. Uncertainties on these reddenings are +/-0.015 for Burstein and Heiles and +/-0.03 for those derived from (V-K). mag r_E(B-V) Reference for E(B-V) number=6 E(B-V) is from (1) Burstein and Heiles (1982AJ.....87.1165B) (2) Using the Log(P)-(V-K) relations discussed in Section 2.2. Uncertainties on these reddenings are +/-0.015 for Burstein and Heiles and +/-0.03 for those derived from (V-K). --- RV Systemic radial velocity number=7 The sources of the data are as follows: 1: Skillen et al., 1993MNRAS.265..301S 2: Fernley et al., 1990MNRAS.247..287F 3: Meylan et al., 1986A&AS...64...25M 4: Liu and Janes 1990, 1990ApJ...354..273L 5: Jones et al., 1988ApJ...332..206J 6: Carrillo et al., 1995A&AS..113..483C, Cat. <J/A+AS/113/483> 7: Cacciari et al., 1987A&AS...69..135C 8: Clementini et al., 1990A&AS...85..865C 9: Solano et al., 1997A&AS..125..321S, Cat. <J/A+AS/125/321> 10: Fernley and Barnes, 1997A&AS..125..313F, Cat. <J/A+AS/125/313> 11: Hawley and Barnes, 1985PASP...97..551H 12: Fernley et al., 1993A&AS...97..815F 13: Layden, 1994AJ....108.1016L, Cat. <J/AJ/108/1016> 14: Woolley and Aly, 1966RGOB..114..259W 15: Kinman, 1961RGOB...37..151K 16: Clube, Evans and Jones, 1969MmRAS..72..101C 17: Breger, 1964MNSSA..23..112B 18: Notni, 1956MiJen..26....1N 19: Joy, 1938PASP...50..302J, 1950PASP...62...60J, 1955PASP...67..420J km/s e_RV rms uncertainty on RV number=7 The sources of the data are as follows: 1: Skillen et al., 1993MNRAS.265..301S 2: Fernley et al., 1990MNRAS.247..287F 3: Meylan et al., 1986A&AS...64...25M 4: Liu and Janes 1990, 1990ApJ...354..273L 5: Jones et al., 1988ApJ...332..206J 6: Carrillo et al., 1995A&AS..113..483C, Cat. <J/A+AS/113/483> 7: Cacciari et al., 1987A&AS...69..135C 8: Clementini et al., 1990A&AS...85..865C 9: Solano et al., 1997A&AS..125..321S, Cat. <J/A+AS/125/321> 10: Fernley and Barnes, 1997A&AS..125..313F, Cat. <J/A+AS/125/313> 11: Hawley and Barnes, 1985PASP...97..551H 12: Fernley et al., 1993A&AS...97..815F 13: Layden, 1994AJ....108.1016L, Cat. <J/AJ/108/1016> 14: Woolley and Aly, 1966RGOB..114..259W 15: Kinman, 1961RGOB...37..151K 16: Clube, Evans and Jones, 1969MmRAS..72..101C 17: Breger, 1964MNSSA..23..112B 18: Notni, 1956MiJen..26....1N 19: Joy, 1938PASP...50..302J, 1950PASP...62...60J, 1955PASP...67..420J km/s r_RV Reference for RV --- [Fe/H] Metallicity number=8 [Fe/H] use the relation [Fe/H]=-0.13-0.195{DELTA}S from Fernley and Barnes (1997, A&AS, in press). Typically the error on these abundances is +/-0.15 dex. Sources of data are as follows: (1) Suntzeff, Kraft and Kinman, 1991ApJ...367..528S (2) Fernley and Barnes, 1997, A&AS, in press (3) Solano et al., 1997, A&AS, in press (4) Lambert et al., 1996ApJS..103..183L (5) Clementini et al., 1995AJ....110.2319C, Cat. <J/AJ/110/2319> (6) Layden, 1994AJ....108.1016L, Cat. <J/AJ/108/1016> (7) Kemper, 1982AJ.....87.1395K (8) Butler, 1975ApJ...200...68B (unless superseded by ref 1) (9) Preston, 1959ApJ...130..507P (unless superseded by ref 1) (10) Kinman and Caretta, 1992PASP..104..111K (11) Smith, 1990PASP..102..124S (12) Clementini et al., 1991AJ....101.2168C (13) Kinman, 1961RGOB...37..151K (14) Clube, Evans and Jones, 1969MmRAS..72..101C [Sun] r_[Fe/H] Reference for [Fe/H] number=8 [Fe/H] use the relation [Fe/H]=-0.13-0.195{DELTA}S from Fernley and Barnes (1997, A&AS, in press). Typically the error on these abundances is +/-0.15 dex. Sources of data are as follows: (1) Suntzeff, Kraft and Kinman, 1991ApJ...367..528S (2) Fernley and Barnes, 1997, A&AS, in press (3) Solano et al., 1997, A&AS, in press (4) Lambert et al., 1996ApJS..103..183L (5) Clementini et al., 1995AJ....110.2319C, Cat. <J/AJ/110/2319> (6) Layden, 1994AJ....108.1016L, Cat. <J/AJ/108/1016> (7) Kemper, 1982AJ.....87.1395K (8) Butler, 1975ApJ...200...68B (unless superseded by ref 1) (9) Preston, 1959ApJ...130..507P (unless superseded by ref 1) (10) Kinman and Caretta, 1992PASP..104..111K (11) Smith, 1990PASP..102..124S (12) Clementini et al., 1991AJ....101.2168C (13) Kinman, 1961RGOB...37..151K (14) Clube, Evans and Jones, 1969MmRAS..72..101C --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1997 Sep 11 John Fernley <JAF@v3600.vilspa.esa.es> UNKNOWN UNKNOWN Of the 180 stars classified by HIPPARCOS as RR Lyraes and observed by the satellite the following stars were removed: CH AQL: No metallicity IN ARA: Poor quality HIPPARCOS data (like RW COL) BH AUR: No reddening BB CMI: Ecl. Var. (Schmidt et al., 1995AJ....109.1239S) V363 CAS: Fourier Coefficient R(21) is unusual - Anom. Ceph (see section 2.3) V753 CEN: Period too short (0.221 days) EZ CEP: Poor quality HIPPARCOS data (like RW COL) XZ CET: Fourier Coefficient R(21) is unusual - Anom. Ceph (see section 2.3) RW COL: HIPPARCOS data are Poor quality (light curve has a lot of scatter and Trig Parallax and Proper Motion have large errors) V1719 CYG: Long period Delta Scuti (Fernley and Barnes, 1997, A&AS, in press) VZ DRA: No metallicity BX DRA: Ecl. Var. (Schmidt et al., 1995AJ....109.1239S) XZ GRU: Period too long (0.883 days) LS HER: Period too short (0.231 days) SZ HYA: Poor quality HIPPARCOS data (like RW COL) BI HYA: Constant V mag from HIPPARCOS photometry ET HYA: Both constant V mag from HIPPARCOS and constant radial velocity from spectra (Fernley and Barnes, 1997, A&AS, in press) CZ LAC: Poor quality HIPPARCOS data (like RW COL) CW LUP: Both constant V mag from HIPPARCOS and constant radial velocity from spectra (Solano et al., 1997, A&AS, in press) TV LYN: Period too short (0.241 days) VY NOR: Poor quality HIPPARCOS data (like RW COL) V429 ORI: Both constant V mag from HIPPARCOS and constant radial velocity from spectra (Fernley and Barnes, 1997, A&AS, in press) IV PAV: Period too short (0.203 days) KN PER: Ecl. Var (Schmidt, 1991AJ....102.1766S) ST PIC: No metallicity or radial velocity SS PSC: Long period Delta Scuti (Fernley and Barnes, 1997, A&AS, in press) IU PUP: Constant V mag from HIPPARCOS photometry KZ PUP: Period too long (2.018 days) V2232 SGR: Poor quality HIPPARCOS data (like RW COL) V494 SCO: No Reddening V690 SCO: No Reddening UY SCL: Period too short (0.182 days) AR SER: Fourier Coefficient R(21) is unusual - Anom. Ceph (see section 2.3) CD VEL: No metallicity or radial velocity BB VIR: Photometric evidence for HB Companion (Fernley, 1993Obs...113..197F) NSV5394: Constant V mag from HIPPARCOS photometry -------------------------------------------------------------------------------- J_A+A_330_515.xml Silicon and sulfur chemistry in the inner wind of IRC+10216 J/A+A/330/676 J/A+A/330/676 IRC+10216 Silicon and sulfur chemistry Silicon and sulfur chemistry in the inner wind of IRC+10216 K Willacy I Cherchneff Astron. Astrophys. 330 676 1998 1998A&A...330..676W Atomic physics Stars, giant molecular processes stars: AGB and post-AGB stars: individual (IRC+10 216) We present a dynamical and chemical model of the inner wind of the carbon-rich, AGB star IRC+10216. We include the effect of pulsation-driven shocks on the gas envelope close to the stellar photosphere and construct an extended chemical model that includes in particular the chemistry of hydrocarbon species and silicon and sulphur-bearing molecules. The derived theoretical abundances for many molecules are in excellent agreement with values obtained from observations of infrared ro-vibrational molecular lines. We confirm the ``parent'' character of certain chemical species and show that the inner wind of IRC+10216, and more generally of evolved AGB stars, is an active dynamical and chemical region where molecules are formed and processed.
IRC +10216 CW Leo 09 47 57.2 +13 16 44
The reaction set Num Sequential number for the reaction --- Reac Reaction --- Dnu {DELTA}{nu} number=1 {nu} is the stochiometric factor --- A Arrhenius A parameter number=2 Rate in the Arrhenius form k = A (T/300)^n^exp(-E/T) Where A has a value of 0.0 the rate is calculated from equation 4 using the parameters for the previous reaction listed. T is the gas kinetic temperature --- n Arrhenius n parameter number=2 Rate in the Arrhenius form k = A (T/300)^n^exp(-E/T) Where A has a value of 0.0 the rate is calculated from equation 4 using the parameters for the previous reaction listed. T is the gas kinetic temperature --- E Arrhenius E parameter number=2 Rate in the Arrhenius form k = A (T/300)^n^exp(-E/T) Where A has a value of 0.0 the rate is calculated from equation 4 using the parameters for the previous reaction listed. T is the gas kinetic temperature K Ref Reference number=3 The references are: R95: Millar et al., 1997A&AS..121..139M ER95: estimated using rates from Millar et al., 1997A&AS..121..139M (The reaction used as the source of the rate is given) CBT: Cherchneff et al., 1992ApJ...401..269C Baulch92: Baulch et al. 1992, J. Phys. Chem. Ref. Data 21, 411 NIST: Mallard et al. 1994, NIST Chemical Kinetics Database: Version 6.0, National Institute of Standards and Technology, Gaithersburg (MD) Mackay: MacKay, 1995MNRAS.274..694M E: an estimated rate for a collider reaction. Those reactions for which the reverse rates are calculated by using thermodynamics are shown by <->, the reverse for all other reactions is given explicitly in the ratefile. --- table5.tex LaTeX version of table5 Patricia Bauer CDS 1997 Sep 22 Isabelle Cherchneff <imc@europa.phy.umist.ac.uk> J_A+A_330_676.xml The H{alpha} kinematics of the Cartwheel galaxy J/A+A/330/881 J/A+A/330/881 Radial velocities of Cartwheel Galaxy The H{alpha} kinematics of the Cartwheel galaxy P Amram C Mendes de Oliveira J Boulesteix C Balkowski Astron. Astrophys. 330 881 1998 1998A&A...330..881A Galaxies, ring Radial velocities galaxies: individual (Cartwheel) galaxies: interactions galaxies: ISM galaxies: kinematics and dynamics galaxies: structure We report on high spectral and spatial resolution kinematic observations of H{alpha} emission from the Cartwheel system obtained with a scanning Fabry-Perot interferometer. Velocity fields for two galaxies were measured, for the main galaxy of the system, the Cartwheel galaxy, and for a spiral companion ~25h^-1^kpc to the north. The velocity field and the rotation curve of the spiral companion shows classical differential rotation and indicates the mass of the galaxy to be in the range 2.9-4.8x10^9^M{sun}. The Cartwheel galaxy contains strong H{alpha} in emission asymmetrically distributed along its outer ring, with some faint emission detected inside it. The velocity field and the rotation curve of the Cartwheel galaxy is clearly dominated by differential rotation although second-order effects cause distortions which can be understood in a scenario where expansion and density-wave motions are also considered. Our best model-fit to the observed velocity field of the Cartwheel galaxy includes three components for the kinematic of its outer ring: a circular velocity of 217km/s, an expansion velocity of 13-30+/-10km/s and a sinusoidal perturbation with an amplitude of 20+/-5km/s. This expansion velocity, lower than found in previous studies, implies that the ring could be older than previously thought. The rotation curve of the Cartwheel galaxy is consistent with a progenitor which had the morphology of a late-type spiral galaxy. Our measurements support the collisional models of ring galaxy formation and should impose strong constraints to simulations.
Cartwheel galaxy ESO 350- 40 00 37 40.7 -33 42 58
Radial characteristics of the Cartwheel (Fig. 5) Radial characteristics for the spiral companion (Fig. 11) Rad Mean radius of the annulus on the major axis arcsec Napp Number of points with measurable radial velocities in this annulus for the approaching side --- Vapp Weighted average velocity calculated from Napp velocity points km/s e_Vapp rms uncertainty on Vapp km/s Nrec Number of points with measurable radial velocities in this annulus for the receding side --- Vrec Weighted average velocity calculated from Nrec velocity points km/s e_Vrec rms uncertainty on Vrec km/s Ntot Total number of velocity points in the annulus Napp+Nrec --- Vel Weighted average velocity calculated from both sides km/s e_Vel rms uncertainty on Vel km/s table3.tex LaTeX version of the tables Patricia Bauer CDS 1997 Aug 20 Philippe Amram <amram@observatoire.cnrs-mrs.fr> J_A+A_330_881.xml Deep optical and near infrared imaging photometry of the Serpens cloud core J/A+A/330/990 J/A+A/330/990 VRIJHK photometry of the Serpens cloud core Deep optical and near infrared imaging photometry of the Serpens cloud core P Giovannetti E Caux D Nadeau J -L Monin Astron. Astrophys. 330 990 1998 1998A&A...330..990G Clusters, open Photometry, infrared Stars, pre-main sequence infrared: stars open clusters and associations: individual (Serpens cloud) stars: formation stars: luminosity function, mass function stars: pre-main sequence We present results from a deep optical (VRI) and near infrared (JHK) survey of the central part of the Serpens molecular cloud. A total of 138 sources were detected in the 19 arcmin^2^ surveyed area down to a limiting magnitude of 16.3 in K. We find that the form of the observed K Luminosity Function (KLF) of stars belonging to the Serpens Molecular cloud is consistent with that predicted from a Miller & Scalo (1979ApJS...41..513M) Interstellar Mass Function (IMF). We have investigated the KLF evolution with the age of a cluster by modeling KLFs of hypothetical clusters. Our results suggest that two phases of star formation could have taken place in the Serpens core.
Log of observations Name Sequential object number --- n_Name S: Serpens cloud members --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec n_Vmag Note on Vmag number=1 x: Regions of the sky that were not observed in the concerned photometric band nd: Sources that were not detected --- Vmag V magnitude mag e_Vmag 3 {sigma} uncertainty on Vmag mag n_Rmag Note on Rmag number=1 x: Regions of the sky that were not observed in the concerned photometric band nd: Sources that were not detected --- Rmag R magnitude mag e_Rmag 3 {sigma} uncertainty on Rmag mag n_Imag Note on Imag number=1 x: Regions of the sky that were not observed in the concerned photometric band nd: Sources that were not detected --- Imag I magnitude mag e_Imag 3 {sigma} uncertainty on Imag mag n_Jmag Note on Jmag number=1 x: Regions of the sky that were not observed in the concerned photometric band nd: Sources that were not detected --- Jmag J magnitude mag e_Jmag 3 {sigma} uncertainty on Jmag mag n_Hmag Note on Hmag number=1 x: Regions of the sky that were not observed in the concerned photometric band nd: Sources that were not detected --- Hmag H magnitude mag e_Hmag 3 {sigma} uncertainty on Hmag mag n_Kmag Note on Kmag number=1 x: Regions of the sky that were not observed in the concerned photometric band nd: Sources that were not detected --- Kmag K magnitude mag e_Kmag 3 {sigma} uncertainty on Kmag mag Other Other identification number=2 CK: Churchwell and Koornneef (1986ApJ...300..729C) EC: Eiroa and Casali (1992A&A...262..468E) GEL: Gomez de Castro et al. (1988A&A...201..299G) HCE: Horrobin et al. (1997A&A...320L..41H) --- table2.tex Latex version of table2 Patricia Bauer CDS 1997 Sep 04 Philippe Giovannetti <Philippe.Giovannetti@cesr.cnes.fr> J_A+A_330_990.xml Rotation and chromospheric activity in field M dwarfs J/A+A/331/581 J/A+A/331/581 Rotation and activity in field M dwarfs Rotation and chromospheric activity in field M dwarfs X Delfosse T Forveille C Perrier M Mayor Astron. Astrophys. 331 581 1998 1998A&A...331..581D Parallaxes, trigonometric Rotaional velocities Space velocities Stars, M-type stars: activity stars: chromospheres stars: coronae stars: low-mass, brown dwarfs stars: rotation We have obtained high resolution spectra for a volume-limited sample of 118 field M dwarfs. From these observations we derive projected rotational velocities and fluxes in the H{alpha} and H{beta} lines. 8 stars are double-lined spectroscopic binaries with measured or probable periods short enough for rotation to be tidally synchronized with the orbit, and another 11 are visual binaries where we cannot yet separate the lines of the two stars. Of the remaining 99 stars, 24 have rotational velocities above our detection limit of ~2km/s, and some are quite fast rotators, including two with vsini>30km/s and one with vsini~50km/s. Given the small radii of M dwarfs, these moderate rotational velocities correspond to rather short maximum rotational periods, of only 7-8 hours.
Basic parameters of the sample stars Name Name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec SpType Spectral type number=1 Spectral type are from Reid et al (1995AJ....110.1838R), except when n_Type=a, then spectral type from Henry et al. (1994AJ....108.1437H). --- n_SpType Note on Spectral type number=1 Spectral type are from Reid et al (1995AJ....110.1838R), except when n_Type=a, then spectral type from Henry et al. (1994AJ....108.1437H). --- R-I R-I color index number=2 The (R-I) is in Cousin system and is from Leggett's (1992ApJS...82..351L) compilation except when n_R-I=b, data from the CNS3 catalog (Gliese and Jahreiss, 1991, Cat. <V/70>; the Kron R-I in the CNS3 were transformed to the Cousins system using the Bessell (1983PASP...95..480B) relation, (R-I)_c=1.20(R-I)_k+0.08); n_R-I=c, data from Bessell (1990A&AS...83..357B); n_R-I=d, data estimated from spectral type, using Leggett's (1992ApJS...82..351L) relation for the Young Disk. mag n_R-I Note on R-I number=2 The (R-I) is in Cousin system and is from Leggett's (1992ApJS...82..351L) compilation except when n_R-I=b, data from the CNS3 catalog (Gliese and Jahreiss, 1991, Cat. <V/70>; the Kron R-I in the CNS3 were transformed to the Cousins system using the Bessell (1983PASP...95..480B) relation, (R-I)_c=1.20(R-I)_k+0.08); n_R-I=c, data from Bessell (1990A&AS...83..357B); n_R-I=d, data estimated from spectral type, using Leggett's (1992ApJS...82..351L) relation for the Young Disk. --- VMAG V Absolute magnitude mag Mbol Bolometric absolute magnitude mag plx Trigonometric parallax mas n_plx Note on Plx number=3 Parallax and proper motion are from e: the Yale General Catalogue of Trigonometric Stellar Parallaxes (Van Altena et al. 1991, see Cat. <I/238>), or f: the Hipparcos input catalogue (Turon et al., 1993, Cat. <I/196>). --- e_plx rms uncertainty on plx mas pmRA Proper motion in RA number=3 Parallax and proper motion are from e: the Yale General Catalogue of Trigonometric Stellar Parallaxes (Van Altena et al. 1991, see Cat. <I/238>), or f: the Hipparcos input catalogue (Turon et al., 1993, Cat. <I/196>). mas/yr pmDE Proper motion in DE number=3 Parallax and proper motion are from e: the Yale General Catalogue of Trigonometric Stellar Parallaxes (Van Altena et al. 1991, see Cat. <I/238>), or f: the Hipparcos input catalogue (Turon et al., 1993, Cat. <I/196>). mas/yr RV Radial velocity km/s Rotational, activity, and kinematics parameters Name Name --- Sig Width of correlation profile number=1 With a K0 template, except when n_sig=a, then with the M0 template. km/s n_Sig Note on Sig number=1 With a K0 template, except when n_sig=a, then with the M0 template. --- e_Sig Standard error on Sig number=2 The quoted uncertainty on Sig is that due to photon and readout noise, while the standard error on vsini also includes a 200m/s dispersion on Sig_0, the width of the correlation profile of a non rotating star km/s l_vsini Limit flag on vsini --- vsini Projected rotational velocities km/s e_vsini Standard error on vsini number=2 The quoted uncertainty on Sig is that due to photon and readout noise, while the standard error on vsini also includes a 200m/s dispersion on Sig_0, the width of the correlation profile of a non rotating star km/s Lbol Logarithm of bolometric luminosities 10-7W LHalpha Logarithm of H{alpha} luminosities 10-7W e_LHalpha rms uncertainty on LHalpha 10-7W LHbeta Logarithm of H{beta} luminosities 10-7W e_LHbeta rms uncertainty on LHbeta 10-7W l_Lx Limit flag on Lx --- Lx Logarithm of the X luminosities number=3 From Schmitt et al. (1995ApJ...450..392S) and the ROSAT all sky survey (Voges et al., 1996, Cat. <IX/10>). 10-7W Uvel Space motion number=4 The UVW space motion are heliocentric, with U positive toward the Galactic anticenter. km/s n_Uvel Note on Uvel number=5 b: space velocities were computed using an inaccurate radial velocity (+/-2km/s), because we have not yet covered a full orbital period. c: space velocities use the barycentric radial velocity from Marcy & Chen (1992ApJ...390..550M). --- Vvel Space motion number=4 The UVW space motion are heliocentric, with U positive toward the Galactic anticenter. km/s n_Vvel Note on Vvel number=5 b: space velocities were computed using an inaccurate radial velocity (+/-2km/s), because we have not yet covered a full orbital period. c: space velocities use the barycentric radial velocity from Marcy & Chen (1992ApJ...390..550M). --- Wvel Space motion number=4 The UVW space motion are heliocentric, with U positive toward the Galactic anticenter. km/s n_Wvel Note on Wvel number=5 b: space velocities were computed using an inaccurate radial velocity (+/-2km/s), because we have not yet covered a full orbital period. c: space velocities use the barycentric radial velocity from Marcy & Chen (1992ApJ...390..550M). --- Pop Dynamic population number=6 The code is: YD: young disk YO: young-old disk OD: old disk OH: old disk-Halo H: Halo --- Patricia Bauer CDS 1997 Nov 13 Xavier Delfosse <Xavier.Delfosse@obs.unige.ch> J_A+A_331_581.xml Identification of Lambda Bootis stars using IUE spectra. I. Low Resolution Data J/A+A/331/633 J/A+A/331/633 IUE spectra of lambda Boo stars Identification of Lambda Bootis stars using IUE spectra. I. Low Resolution Data E Solano E Paunzen Astron. Astrophys. 331 633 1998 1998A&A...331..633S J/A+AS/123/93 : Lambda Boo stars consolidated catalogue (Paunzen+ 1997) Spectra, ultraviolet Stars, early-type Stars, peculiar stars: chemically peculiar stars: early-type ultraviolet: stars An analysis of the stars included in the catalogue of {lambda} Bootis stars by Paunzen et al. (1997, Cat. <J/A+AS/123/93>) and which also have IUE observations is presented here. Population I A-F type stars as well as field horizontal branch stars were also included in the analysis. Using line-ratios of carbon to heavier elements (Al and Ni) allows us to establish unambiguous membership criteria for the {lambda} Bootis group.
Lambda Bootis stars included in Paper I (Pauzen et al., 1997, Cat. <J/A+AS/123/93>) with ultraviolet observations Same as table1.dat but for the field horizontal branch stars Same as table1.dat but for the standard stars Name Star identification --- Teff Effective temperature (this work) K Teff2 Effective temperature from other work number=1 Sources for T_eff_: 1: Iliev & Barzova (1995A&A...302..735I) 2: Stuerenburg (1993A&A...277..139S) 3: Venn & Lambert (1990ApJ...363..234V) 4: North et al. (1994A&A...281..775N) 5: Cacciari et al. (1987A&A...183..314C) 6: Huenemoerder et al. (1984AJ.....89..851H) 7: De Boer et al. (1997A&A...317L..23) 8: Adelman & Philip (1990MNRAS.247..132A) 9: Hayes & Philip (1988PASP..100..801H) 11: Holweger & Rentzsch-Holm (1995A&A...303..819H) 12: Smalley & Dworetsky (1995A&A...293..446S) 13: Blackwell & Lynas-Gray (1994, Cat. <J/A+A/282/899>) 14: Alonso et al. (1996A&A...313..873A) 15: Malagnini & Morossi (1990A&AS...85.1015M) 16: Smalley (1993MNRAS.265.1035S) 17: Smalley & Dworetsky (1993A&A...271..515S) 18: Napiwotzki et al. (1993A&A...268..653N) 19: Adelman et al. (1980ApJS...43..491A) 20: Nissen (1981A&A....97..145N) 21: Van Veer-Menneret et al. (1989A&A...224..171V) 22: Hill & Landstreet (1993, Cat. <J/A+A/276/142>) 23: Gerbaldi et al. (1989A&AS...81..127G) 24: Adelman (1978ApJ...222..547A) K r_Teff2 Reference for Teff2 --- Teff3 Effective temperature from other work number=1 Sources for T_eff_: 1: Iliev & Barzova (1995A&A...302..735I) 2: Stuerenburg (1993A&A...277..139S) 3: Venn & Lambert (1990ApJ...363..234V) 4: North et al. (1994A&A...281..775N) 5: Cacciari et al. (1987A&A...183..314C) 6: Huenemoerder et al. (1984AJ.....89..851H) 7: De Boer et al. (1997A&A...317L..23) 8: Adelman & Philip (1990MNRAS.247..132A) 9: Hayes & Philip (1988PASP..100..801H) 11: Holweger & Rentzsch-Holm (1995A&A...303..819H) 12: Smalley & Dworetsky (1995A&A...293..446S) 13: Blackwell & Lynas-Gray (1994, Cat. <J/A+A/282/899>) 14: Alonso et al. (1996A&A...313..873A) 15: Malagnini & Morossi (1990A&AS...85.1015M) 16: Smalley (1993MNRAS.265.1035S) 17: Smalley & Dworetsky (1993A&A...271..515S) 18: Napiwotzki et al. (1993A&A...268..653N) 19: Adelman et al. (1980ApJS...43..491A) 20: Nissen (1981A&A....97..145N) 21: Van Veer-Menneret et al. (1989A&A...224..171V) 22: Hill & Landstreet (1993, Cat. <J/A+A/276/142>) 23: Gerbaldi et al. (1989A&AS...81..127G) 24: Adelman (1978ApJ...222..547A) K r_Teff3 Reference for Teff3 --- Teff4 Effective temperature from other work number=1 Sources for T_eff_: 1: Iliev & Barzova (1995A&A...302..735I) 2: Stuerenburg (1993A&A...277..139S) 3: Venn & Lambert (1990ApJ...363..234V) 4: North et al. (1994A&A...281..775N) 5: Cacciari et al. (1987A&A...183..314C) 6: Huenemoerder et al. (1984AJ.....89..851H) 7: De Boer et al. (1997A&A...317L..23) 8: Adelman & Philip (1990MNRAS.247..132A) 9: Hayes & Philip (1988PASP..100..801H) 11: Holweger & Rentzsch-Holm (1995A&A...303..819H) 12: Smalley & Dworetsky (1995A&A...293..446S) 13: Blackwell & Lynas-Gray (1994, Cat. <J/A+A/282/899>) 14: Alonso et al. (1996A&A...313..873A) 15: Malagnini & Morossi (1990A&AS...85.1015M) 16: Smalley (1993MNRAS.265.1035S) 17: Smalley & Dworetsky (1993A&A...271..515S) 18: Napiwotzki et al. (1993A&A...268..653N) 19: Adelman et al. (1980ApJS...43..491A) 20: Nissen (1981A&A....97..145N) 21: Van Veer-Menneret et al. (1989A&A...224..171V) 22: Hill & Landstreet (1993, Cat. <J/A+A/276/142>) 23: Gerbaldi et al. (1989A&AS...81..127G) 24: Adelman (1978ApJ...222..547A) K r_Teff4 Reference for Teff4 --- log(g) Surface gravity [cm/s2] r_log(g) Reference for log(g) number=2 Sources for log(g): 6: Huenemoerder et al. (1984AJ.....89..851H) 9: Hayes & Philip (1988PASP..100..801H) nothing: this work --- Images IUE Images (SWP/LWP). number=3 Camera and image number. The L and S following the image number indicates the aperture used (Large or Small) ----- EW(1657/2800) Equivalent width at 1657/2800A 0.1nm EW(1670) Equivalent width at 1670A 0.1nm EW(1741) Equivalent width at 1741A 0.1nm EW(1931) Equivalent width at 1931A 0.1nm tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Nov 04 Enrique Solano <ESM@vilspa.esa.es> J_A+A_331_633.xml Infrared Array Photometry of Bulge Globular Clusters. I. Combined ground based JK and HST VI Photometry of NGC 6553 J/A+A/331/70 J/A+A/331/70 JKVI photometry of NGC 6553 stars Infrared Array Photometry of Bulge Globular Clusters. I. Combined ground based JK and HST VI Photometry of NGC 6553 M D Guarnieri S Ortolani P Montegriffo A Renzini B Barbuy E Bica A Moneti Astron. Astrophys. 331 70 1998 1998A&A...331...70G Clusters, globular Photometry, infrared Stars, blue blue stragglers Galaxy: center globular clusters: individual (NGC 6553) Hertzsprung-Russell (HR diagram) JK infrared photometry for the bulge globular cluster NGC 6553, combined with high resolution visual VI observations are presented and discussed in connection with the bulge metal rich population. The infrared data were taken with IRAC2 at ESO 2.2m telescope while the optical counterparts are from Hubble Space Telescope (HST). We find a mean magnitude for the horizontal branch of V_HB_=16.92, and K_HB_=12.42+/-0.01. Assuming a reddening of E(B-V)=0.7, the mean distance modulus is (m-M)_0_=13.6 giving an heliocentric distance of 5.2Kpc. This distance is slightly higher than that previously published by Ortolani et al. (1990A&A...236..362O, hereafter OBB90). The brightest giants have been detected at K~6.5 and (V-K)=13.10 transforming to M_K_=-7.34 and (V-K)_0_=11.20, which are exceptionally high values for a globular cluster. The metallicity has been found to be consistent with previous values and an average of [Fe/H]=-0.22+/-0.05 has been adopted. The helium abundance estimated via the R' method yields Y_p_~0.28+/-0.03.
NGC 6553 18 09 15.6 -25 54 28
VIJK photometry of 1426 stars No Sequential number number=1 No 1 to 2197 belong to the WFPC2 PC chip 20001 to 26240 to the WFPC2 chip#2 30001 to 39545 to the WFPC2 chip#3 40001 to 48688 to the WFPC2 chip#4 --- Vmag HST V magnitude mag Imag HST I magnitude mag Jmag IRAC2 J magnitude mag Kmag IRAC2 K magnitude mag Xpos HST X position number=2 X position transformed to the IRAC2 reference frame pix Ypos HST Y position pix Patricia Bauer CDS 1997 Sep 09 UNKNOWN UNKNOWN Prepared via OCR at CDS from the manuscript. J_A+A_331_70.xml The Hyades: distance, structure, dynamics, and age J/A+A/331/81 J/A+A/331/81 Hyades membership The Hyades: distance, structure, dynamics, and age M A C Perryman A G A Brown Y Lebreton A Gomez C Turon G Cayrel de Strobel J C Mermilliod N Robichon J Kovalevsky F Crifo Astron. Astrophys. 331 81 1998 1998A&A...331...81P I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Clusters, open Parallaxes, trigonometric Radial velocities Stars, distances astrometry distance scale Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Hyades) parallaxes We use absolute trigonometric parallaxes from the Hipparcos Catalogue (Cat. <I/239>) to determine individual distances to members of the Hyades cluster, from which the 3-dimensional structure of the cluster can be derived. Inertially-referenced proper motions are used to rediscuss distance determinations based on convergent-point analyses. A combination of parallaxes and proper motions from Hipparcos, and radial velocities from ground-based observations, are used to determine the position and velocity components of candidate members with respect to the cluster centre, providing new information on cluster membership: 13 new candidate members within 20pc of the cluster centre have been identified. Farther from the cluster centre there is a gradual merging between certain cluster members and field stars, both spatially and kinematically. Within the cluster, the kinematical structure is fully consistent with parallel space motion of the component stars with an internal velocity dispersion of about 0.3km/s. The spatial structure and mass segregation are consistent with N-body simulation results, without the need to invoke expansion, contraction, rotation, or other significant perturbations of the cluster. The quality of the individual distance determinations permits the cluster zero-age main sequence to be accurately modelled. The helium abundance for the cluster is determined to be Y=0.26+/-0.02 which, combined with isochrone modelling including convective overshooting, yields a cluster age of 625+/-50Myr. The distance to the observed centre of mass (a concept meaningful only in the restricted context of the cluster members contained in the Hipparcos Catalogue) is 46.34+/-0.27pc, corresponding to a distance modulus m-M=3.33+/-0.01mag for the objects within 10pc of the cluster centre (roughly corresponding to the tidal radius). This distance modulus is close to, but significantly better determined than, that derived from recent high-precision radial velocity studies, somewhat larger than that indicated by recent ground-based trigonometric parallax determinations, and smaller than those found from recent studies of the cluster convergent point. These discrepancies are investigated and explained.
Data on the membership of the Hyades for the 282 stars in the sample of Perryman et al. HIP Hipparcos Catalogue (HIP, Cat. <I/239>) number --- vB van Bueren number (1952BAN....11..385V) --- n_vB n: new candidate proposed in this paper --- MembvB Membership according to van Bueren number=1 Data on the membership of the Hyades for the 282 stars in our sample, listed by various authors. Membership or non-membership inferred by the relevant authors are indicated by `1' or `0' in the corresponding column respectively (see paper for details). --- vA van Altena number (1969AJ.....74....2V) --- n_vA n: new candidate proposed in this paper --- MembvA Membership according to van Altena number=1 Data on the membership of the Hyades for the 282 stars in our sample, listed by various authors. Membership or non-membership inferred by the relevant authors are indicated by `1' or `0' in the corresponding column respectively (see paper for details). --- Han Hanson number (1975, Cat. <J/AJ/80/379>) --- n_Han n: new candidate proposed in this paper --- MembHan Membership according to Hanson number=1 Data on the membership of the Hyades for the 282 stars in our sample, listed by various authors. Membership or non-membership inferred by the relevant authors are indicated by `1' or `0' in the corresponding column respectively (see paper for details). --- Pel Pels et al. (1975A&A....43..423P) (Leiden) number, van Bueren stars have the vB number + 1000 --- n_Pel n: new candidate proposed in this paper --- MembPel Membership according to Pels et al. number=1 Data on the membership of the Hyades for the 282 stars in our sample, listed by various authors. Membership or non-membership inferred by the relevant authors are indicated by `1' or `0' in the corresponding column respectively (see paper for details). --- Grif Sequential number in Table4 of Griffin et al. (1988AJ.....96..172G) --- n_Grif n: new candidate proposed in this paper --- MembGrif Membership according to Griffin et al. number=1 Data on the membership of the Hyades for the 282 stars in our sample, listed by various authors. Membership or non-membership inferred by the relevant authors are indicated by `1' or `0' in the corresponding column respectively (see paper for details). --- Scha Schwan number (1991A&A...243..386S) --- n_Scha n: new candidate proposed in this paper --- MembScha Membership according to Schwan number=1 Data on the membership of the Hyades for the 282 stars in our sample, listed by various authors. Membership or non-membership inferred by the relevant authors are indicated by `1' or `0' in the corresponding column respectively (see paper for details). --- plx Hipparcos parallax (milliarcsec=mas) mas e_plx Hipparcos parallax standard error mas RV Radial velocity km/s u_RV Uncertainty flag on RV --- n_RV # indicates SB/RV with undetermined gamma velocity --- e_RV Error in radial velocity km/s r_RV Source of radial velocity number=2 Sources of radial velocities: (0) Radial velocity unknown; (1) Griffin et al., 1988AJ.....96..172G 1985AJ.....90..609G 1981AJ.....86..588G 1978AJ.....83.1114G 1977AJ.....82..176G 1982A&A...106..221G (2) Hipparcos Input Catalogue, Cat. <I/196> (mainly from R.E. Wilson, 1953, Cat. <III/21>) (3) Weighted mean of ref. 2 (39.6+/-1.2) and Kraft, 1965ApJ...142..681K (38.4+/-1.5) (4) Kraft, 1965ApJ...142..681K (37.4+/-0.4 and 36.5+/-0.5) Cheriguene, 1971A&A....13..447C (37.3+/-0.7) (5) McClure, 1982ApJ...254..606M (6) Torres et al., 1997ApJ...474..256T (7) Mayor & Mazeh, 1987A&A...171..157M (8) Kraft, 1965ApJ...142..681K (9) Margoni et al., 1992A&AS...93..545M (10) Lucy & Sweeney, 1971AJ.....76..544L (11) Abt & Levy, 1985ApJS...59..229A (12) Griffin, 1971MNRAS.155....1G (13) Andersen & Nordstrom, 1983A&A...122...23A (14) Morse et al., 1991AJ....101.1495M (15) Detweiler et al., 1984AJ.....89.1038D (16) Weighted mean of data from Palmer et al., 1968RGOB..135..385P and Stillwell, 1948PDAO....7..337S (17) Tomkin et al., 1995AJ....109..780T (18) Heintz, 1981ApJS...46..247H (19) Abt, 1965ApJS...11..429A (20) Fekel, 1980PASP...92..785F (21) Perraud, 1962JO.....45..361P (22) Fouts & Sandage, 1986AJ.....91.1189F, Cat. <III/144> (star G83-18) (23) Strassmeier et al., 1988A&AS...72..291S, See Cat. <V/76> (24) New Coravel observations provided by J.C. Mermilliod (25) Woolley et al., 1971ROAn...14....1W (26) Hanson & Vasilevskis, 1983AJ.....88..844H (27) Evans, 1978BICDS..15..121E (28) Orbit recomputed by Mermilliod with period=490+/-1d (from Batten) --- Note SB: spectroscopic binary, RV: radial velocity (possibly) variable --- Note2 Historical status flag number=3 Star was previously known, or classified by Hipparcos, to have resolved components (from Field H56, Cat. <I/239>); this may overlap with the flag in the next column, but may also indicate visual or wide binary (see paper for details) H : determined multiple by Hipparcos, previously unknown I : system previously identified as multiple in HIC <I/196> (annex1) M : miscellaneous (system identified after publication of HIC) --- Note3 Double/Multiple Systems flag number=4 C, G, O, V, or X = relevant part of the Hipparcos Double and Multiple Systems Annex, from Field H59 (Cat. <I/239>), C: solutions for the components G: acceleration or higher order terms O: orbital solutions V: variability-induced movers (apparent motion arises from variability) X: stochastic solution (probably astrometric binaries with short period) supplemented by S = suspected binary in Hipparcos Catalogue, from Field H61, Cat. <I/239>, (see paper for details) --- Dist Distance from the cluster centre defined by the 134 stars within r<10 pc (see Table 3) pc Stat Kinematic statistic number=5 A value of 14.16 corresponding to 3{sigma}, see paper for details. --- Memb Final membership assigned in this paper `?' indicates possible new members unclassifiable due to unknown radial velocities --- Patricia Bauer CDS 1997 Jul 24 Anthony Brown <brown@strw.LeidenUniv.nl> J_A+A_331_81.xml Wolf-Rayet stars and O-star runaways with HIPPARCOS. I. Kinematics. (Based on data from the ESA Hipparcos astrometry satellite) J/A+A/331/949 J/A+A/331/949 Wolf-Rayet and O-star runaways kinematics Wolf-Rayet stars and O-star runaways with HIPPARCOS. I. Kinematics. (Based on data from the ESA Hipparcos astrometry satellite) A F J Moffat S V Marchenko W Seggewiss K A van der Hucht H Schrijver B Stenholm I Lundstrom D Y A Setia Gunawan W Sutantyo E P J van den Heuvel J -P De Cuyper A E Gomez Astron. Astrophys. 331 949 1998 1998A&A...331..949M I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Proper motions Radial velocities Stars, O Stars, Wolf-Rayet astrometry Galaxy: kinematics and dynamics stars: early-type stars: kinematics stars: Wolf-Rayet Reliable systemic radial velocities are almost impossible to secure for Wolf-Rayet stars, difficult for O stars. Therefore, to study the motions - both systematic in the Galaxy and peculiar - of these two related types of hot, luminous star, we have examined the Hipparcos proper motions of some 70 stars of each type. We find that (a) both groups follow Galactic rotation in the same way, (b) both have a similar fraction of ``runaways'', (c) mean kinetic ages based on displacement and motion away from the Galactic plane tend to slightly favour the cluster ejection over the the binary supernova hypothesis for their formation, and (d) those with significant peculiar supersonic motion relative to the ambient ISM, tend to form bow shocks in the direction of the motion.
Summary of pertinent data for peculiar motions of the 74 O stars and 67 WR stars, in order of HIP number (RA for most stars) HD/DM HD/DM catalogue number --- Other Other names --- HIP HIPPARCOS catalogue number (Cat. <I/239>) --- Sp Spectral class --- Vmag Visual magnitude number=1 Broadband Hp V for OB stars, narrowband continuum v for W-R stars. mag GLON Galactic longitude (Epoch 1991.25) deg GLAT Galactic latitude (Epoch 1991.25) deg r Sun-star distance kpc z Star-Galactic plane distance pc pmGLON Observed proper motion (component along the Galactic longitude) mas/yr e_pmGLON Error of pmGLON mas/yr pmGLAT Observed proper motion (component along the Galactic latitude) mas/yr e_pmGLAT Error of pmGLAT mas/yr pmGLONp Peculiar proper motion (component along the Galactic longitude) mas/yr pmGLONp/e_pmGLONp Ratio of the peculiar longitudinal proper motion to the proper motion error --- pmGLATp Peculiar proper motion (component along the Galactic latitude) mas/yr pmGLATp/e_pmGLATp Ratio of the peculiar latitudinal proper motion to the proper motion error --- TVp Peculiar tangential velocity km/s e_TVp Error of the peculiar tangentional velocity km/s HRV Heliocentric radial velocity km/s HRVp Peculiar component of the radial velocity km/s Remarks Comments ---- table1.tex LaTeX version of table1 Patricia Bauer CDS 1999 Apr 23 Sergey Marchenko <sergey@ASTRO.UMontreal.CA> UNKNOWN UNKNOWN On 23-Apr-1999, table1 have been modified and corrected figures 1 to 5 added, see the Erratum 1999A&A...344..321M. J_A+A_331_949.xml Evidence for very large-scale coherent orientations of quasar polarization vectors J/A+A/332/410 J/A+A/332/410 Quasar polarization Evidence for very large-scale coherent orientations of quasar polarization vectors D Hutsemekers Astron. Astrophys. 332 410 1998 1998A&A...332..410H Polarization QSOs large-scale structure of universe methods: statistical polarization quasars: general The table contains optical polarization data for a sample of 170 moderate to high-redshift quasars
The sample of 170 polarized quasars Name Quasar name/position --- GLAT Galactic latitude deg z Redshift --- Pol Polarization degree % e_Pol Uncertainty of polarization degree % PA Polarization position angle deg e_PA Uncertainty of polarization position angle deg Ref References number=1 0: Hutsemekers D., Lamy H., Remy M. 1998, in preparation 1: Berriman G., Schmidt G.D., West S.C., et al., 1990ApJS...74..869B 2: Stockman H.S., Moore R.L., Angel J.R.P., 1984ApJ...279..485S 3: Moore R.L., Stockman H.S., 1984ApJ...279..465M 4: Impey C.D., Tapia S., 1990ApJ...354..124I 5: Impey C.D., Lawrence C.R., Tapia S., 1991ApJ...375...46I 6: Wills B.J., Wills D., Breger M., et al., 1992ApJ...398..454W --- Hutsemekers Liege Astrophysical Institute 1997 Dec 26 Damien Hutsemekers <hutsemek@astro.ulg.ac.be> J_A+A_332_410.xml The fine structure of the Pleiades luminosity function and pre-main sequence evolution J/A+A/332/575 J/A+A/332/575 Pleiades member list The fine structure of the Pleiades luminosity function and pre-main sequence evolution A N Belikov S Hirte H Meusinger A E Piskunov E Schilbach Astron. Astrophys. 332 575 1998 1998A&A...332..575B I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) J/A+A/299/696 : Pleiades field Membership probabilities (Schilbach+, 1995) Mermilliod, J.-C., 1988BICDS..35...77M Mermilliod, J.-C., 1992BICDS..40..115M Clusters, open Proper motions open clusters and associations: individual (Pleiades) stars: luminosity function, mass function stars: pre-main sequence This catalogue contains a list of the Pleiades stars used for the construction of the luminosity function. Additional 24 bright members were taken from the BDA (Mermilliod, 1988BICDS..35...77M, 1992BICDS..40..115M) The corresponding data could be retrieved from the BDA according their designations provided below: BDA-No.: 298, 447, 468, 541, 559, 563, 785, 717, 859, 956, 980, 1306, 1338, 1375, 1380, 1432, 1823, 2168, 2181, 2507, 2690, 3313, 3317, 3327. The catalogue includes 737 cluster members selected on the basis of proper motion and photometric criteria as it is described by Belikov et. al (1998A&A...332..575B). Only 622 "inner" members (with radial distance from the cluster center less than 111.68 arcmin), indicated with spflag=1 were used for the LF construction. 277 stars (n_Vmag=1) have photoelectric V magnitudes from BDA, for the rest (n_Vmag=0) the photographic magnitudes from Schilbach et al. (1995, Cat. <J/A+A/299/696>) survey were used. The luminosity function (LF) of the Pleiades cluster stars was constructed for the study of the LF fine structure related to pre-main sequence (MS) stellar evolution. Theoretical luminosity functions based on present-day pre-MS and MS stellar models were constructed and compared with observations. We tested both power- and log-normal laws describing the cluster star Initial Mass Function (IMF). Both single star formation burst- and age spread-models were examined. The agreement between the observed Pleiades colour-magnitude diagram with the new HIPPARCOS distance and the theoretical ZAMS for a normal metallicity is excellent when the model positions in the HR diagram are corrected to the helium abundance Y=0.34. The corresponding age of the cluster is logt=7.95. Three features (dips) were found in the observed cluster LF in a magnitude range M_V_=5-12mag. Two of them (at M_V_=7.5mag and 9.5mag) are assumed to be field LF features: Wielen and Kroupa dips. Theoretical models fail to reproduce them. We attributed the third (brightest) detail (the dip at M_V_=5.5mag) to the pre-MS evolution of Pleiades stars. The observed Pleiades LF corresponds in its brighter part to the standard Population I IMF. The log-normal IMF fits the observations much better than a simple power-law IMF. The brightest LF feature could be reproduced in the theoretical LF if a substantial age spread of order of several tens of Myrs is supposed to exist among the Pleiades stars.
Star member list in the Pleiades SRS95 Star number from Schilbach et al. (1995, Cat. <J/A+A/299/696>) --- spflag Spatial position flag number=1 1: radial distance less than 111.68 arcmin 0: radial distance greater than or equal to 111.68 arcmin --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec pmRA Proper motion along right ascension direction mas/yr e_pmRA Error in proper motion pmRA mas/yr pmDE Proper motion along declination axis mas/yr e_pmDE Error in proper motion pmDE mas/yr Vmag V magnitude mag n_Vmag Magnitude type flag number=2 1: photoelectric V-mags taken from BDA 0: photographic V-mags taken from Schilbach et al. (1995, Cat. <J/A+A/299/696>) survey --- member Proper motion membership probability --- BDA Star number in the BDA, Mermilliod (1988BICDS..35...77M, 1992BICDS..40..115M) --- Patricia Bauer CDS 1998 Apr 02 Anatoly Piskunov <apiskunov@aip.de> J_A+A_332_575.xml Studies of the flickering in cataclysmic variables. IV. Wavelet transforms of flickering light curves J/A+A/332/586 J/A+A/332/586 Cataclysmic variables light curves Studies of the flickering in cataclysmic variables. IV. Wavelet transforms of flickering light curves T Fritz A Bruch Astron. Astrophys. 332 586 1998 1998A&A...332..586F V/99 : Cataclysmic Binaries and LMXB Catalogue (Ritter+ 1998) Binaries, cataclysmic Photometry binaries: close methods: data analysis novae, cataclysmic variables Wavelet transforms of a large quantity of light curves of numerous CVs in different photometric states were performed in order to quantify the behaviour of the flickering in a statistically significant sample of systems. The scalegram is used as the appropriate tool to describe the wavelet coefficients of stochastically variable data as a function of the time scale. The (logarithmic) scalegram being largely linear for all light curves shows that flickering is a self-similar process and permits a parametrization in terms of its inclination {alpha} and its value {SIGMA} (flickering strength) at a reference time scale. For a given system, {alpha} and {SIGMA} are stable over many years but can vary over shorter periods and are then loosely correlated. On average flickering on short time scales is somewhat bluer than on longer scales. CVs of different types (and photometric states) occupy distinct regions in the {alpha}-{SIGMA}-plane. This behaviour is particularly clear cut for novalike variables where UX UMa stars overlap only slightly with VY Scl stars, and magnetic CVs populate a small range well separated from the other systems. The intrinsic flickering amplitudes of most dwarf novae vary around the outburst cycle with the square root of the system brightness. In dwarf novae with a strong orbital hump the inclination of the scalegram steepens during the outburst. Due probably to complex functional dependences between observable quantities, the physical origins of the flickering, and dynamical system parameters, no clear correlation (only some trends) between flickering characteristics and dynamical or geometrical properties of the CVs can be seen.
List of light curves Name Star name according to the General Catalogue of Variable Stars (Cat. <II/172>) --- Type Type number=1 Photometric type of the system N = classical nova RN = recurrent nova NL = novalike variable UG = dwarf nova --- subType Subtype number=2 Photometric subtype: A = fast nova B = slow nova VY = VY Scl star UX = UX UMa star AC = AM CVn star SS = SS Cyg star SU = SU UMa star WZ = WZ Sge star Z = Z Cam star --- magType Magnetic type number=3 Magnetic types: blanc = non-magnetic system (or unknown) DQ = DQ Her star (intermediate polar) AM = AM Her star (polar) --- Date Date "DD/MM/YY" MJD Modified Julian date (MJD=JD-2400000.5) d PhotState Photometric state number=4 Photometric state - = normal state in those systems which do not exhibit different states (novalike variables and novae; outbursts of the latter are not considered here), or unknown photometric state Q = quiescence (dwarf novae in general) R = rise to outburst (dwarf novae in general) M = outburst maximum (dwarf novae in general) D = decline from outburst (dwarf novae in general) O = unspecified outburst state (dwarf novae in general) S = standstill (Z Cam stars) SM = supermaximum (SU UMa stars) H = high state (VY Scl stars) L = low state (VY Scl stars) --- PhotSys Photometric system number=5 Photometric systems: UBVRI : UBVRI photometry UBVRI*: Stiening system UV : UV photometry white : white light photometry --- Dur Duration of the light curve min TimeRes Time resolution s Band Photometric band number=6 In the case of multicolour photometric systems the photometric band is indicated to which the subsequent columns refer --- SIGMA Scalegram parameter Sigma (see main paper) --- e_SIGMA rms uncertainty on SIGMA --- alpha Scalegram parameter alpha (see main paper) --- e_alpha rms uncertainty on alpha --- mag Mean magnitude during the observations number=7 For light curves in uncalibrated photometric systems a rough estimate from visual observations is given, otherwise mean magnitudes and standard deviations corresponding to the respective photometric band are quoted. mag e_mag rms uncertainty on mag mag table1.tex LaTeX version of the table Patricia Bauer CDS 1998 Mar 05 Albert Bruch <albert@marina.lna.br> J_A+A_332_586.xml The PL relation of galactic carbon LPVs. The distance modulus to LMC J/A+A/332/L53 J/A+A/332/L53 The PL relation of galactic carbon LPVs The PL relation of galactic carbon LPVs. The distance modulus to LMC J Bergeat A Knapik B Rutily Astron. Astrophys. 332, L53 ??? ??? 1998 1998A&A...332L..53B III/156 : Cool Galactic Carbon Stars, 2nd Edition (Stephenson 1989) Parallaxes, trigonometric Stars, carbon galaxies: distances and redshifts stars: AGB and post-AGB stars: carbon stars: fundamental parameters The estimated true parallaxes of 115 carbon LPVs and their unbiased y-values (see Sect. 4) for a study of the period-luminosity relation. The tables contains the entry in the cited Stephenson's catalogue (1989, Cat. <III/156>), the log of the period in days, the absolute magnitude in the K-band, the y-quantity as defined in Sect. 4, the difference between the estimated true parallax and the observed one, the estimated true parallax, the square root of the weight (times 100) of every used y-value for Sample 1 PL-relation (Sect. 4) and the classification into three samples (see Subsec. 3.1).
The data for 115 carbon LPVs GCCS Stephenson's Catalogue (Cat. <III/156>) entry --- logPer The log of the period in days [d] KMag Absolute magnitude in K mag y The y-quantity as defined in Sect. 4 --- Dvarpi True minus Observed parallax mas varpi Estimated true parallax mas 100w Square root of weight x 100 --- S Three samples classification --- u_S Suffix (:) for doubtful S-classification --- table1.ps Post-Script version of the table table1.tex LaTeX version of the table Patricia Bauer CDS J. Bergeat CRAL-Observatoire de Lyon 1998 Feb 19 Jacques BERGEAT <jb@cumulus.univ-lyon1.fr> J_A+A_332_L53.xml Photospheric and chromospheric activity in the late-type giant component of the evolved binary system HD 185510 J/A+A/333/205 J/A+A/333/205 HD 185510 UBV photometry Photospheric and chromospheric activity in the late-type giant component of the evolved binary system HD 185510 A Frasca E Marilli S Catalano Astron. Astrophys. 333 205 1998 1998A&A...333..205F Photometry, UBV Stars, giant Stars, late-type binaries: eclipsing stars: activity stars: individual (HD 185510) subdwarfs UBV photometry and moderate resolution H{alpha} spectrophotometry of the evolved binary system HD 185510 (sdB + K0 III), performed at Catania Astrophysical Observatory, is presented and discussed. The spectrophotometric data were collected in 1991, 1993, and 1994, while the photometric light curves were obtained in 1993, 1994 and 1995. From the B and V photometry we determine a new photometric rotational period of 26.23d, confirming the asynchronous rotation of the cool giant component. The spectroscopic data confirm the vsin i value of 15km/s measured by Fekel et al. (1993AJ....106.2370F) and clearly reveal a filled-in H{alpha} line with appreciable variations. The excess emission of the line, observed at any orbital phase, is found to be anticorrelated with the V light curve and is primarily ascribed to the chromospheric activity on the cool star. The primary total eclipse is clearly visible in the U band, but undetectable in the V band. From the U observations we determined a total duration of the primary eclipse (from 1^st^ to 4^rd^ contact) of 1.3883d, with the ingress lasting only 27 minutes. This new accurate monitoring and timing of the eclipse allowed us to improve the system solution which leads to R_C_=8.8R_{sun}_, T_C_=4800K, R_H_=0.11R_{sun}_, T_H_=30000K for the cool and hot star respectively. The evolution of HD 185510B is discussed also in relation to the evolutionary status of HD 185510A and the synchronization time scale. HD 185510B is probably a sdB near the zero age extended horizontal branch, resulting from an enhanced mass loss in late case B or case A mass exchange with a possible common envelope phase. A small amount (15-20%) of mass loss from the system which can account for the strong IR excess is suggested.
HD 185510 19 39 38.6 -06 03 48
UBV photometry HJD Heliocentric Julian date d Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag e_Vmag rms uncertainty on Vmag mag e_B-V rms uncertainty on B-V mag e_U-B rms uncertainty on U-B mag Npt Number of points contributing to each listed average value number=1 We have listed nightly means of UBV observations far from the ingress or egresses eclipse phases. --- Patricia Bauer CDS 1998 Feb 05 Antonio Frasca <AFRASCA@alpha4.ct.astro.it> J_A+A_333_205.xml Model atmospheres broad-band colors, bolometric corrections and temperature calibrations for O - M stars J/A+A/333/231 J/A+A/333/231 O-M stars model atmospheres Model atmospheres broad-band colors, bolometric corrections and temperature calibrations for O - M stars M S Bessell F Castelli B Plez Astron. Astrophys. 333 231 1998 1998A&A...333..231B VI/39 : Model Atmospheres (Kurucz, 1979) Kurucz, R.L. 1993, "ATLAS9 Stellar Atmosphere Programs and 2 km/s grid", CD-ROM No 13 Models, atmosphere Photometry, UBVRIJKLMNH stars: atmospheres stars: fundamental parameters stars: general Broad band colors and bolometric corrections in the Johnson-Cousins-Glass system (Bessell, 1990PASP..102.1181B; Bessell & Brett, 1988PASP..100.1134B) have been computed from synthetic spectra from new model atmospheres of Kurucz (1995a, priv. comm.), Castelli (1997, priv. comm.), Plez, Brett & Nordlund (1992A&A...256..551P), Plez (1995-97, priv. comm.), and Brett (1995A&A...295..736B, 1995A&AS..109..263B). These atmospheres are representative of larger grids that are currently being completed. We discuss differences between the different grids and compare theoretical color-temperature relations and the fundamental color temperature relations derived from: (a) the infrared-flux method (IRFM) for A-K stars (Blackwell & Lynas-Gray 1994A&A...282..899B; Alonso et al. 1996A&AS..117..227A) and M dwarfs (Tsuji et al. 1996A&A...305L...1T); (b) lunar occultations (Ridgway et al. 1980ApJ...235..126R) and (c) Michelson interferometry (Di Benedetto & Rabbia 1987A&A...188..114D; Dyck et al. 1996AJ....111.1705D; Perrin et al. 1998A&A...331..619P) for K-M giants, and (d) eclipsing binaries for M dwarfs. We also compare color-color relations and color-bolometric correction relations and find good agreement except for a few colors. The more realistic fluxes and spectra of the new model grids should enable accurate population synthesis models to be derived and permit the ready calibration of non-standard photometric passbands. As well, the theoretical bolometric corrections and temperature-color relations will permit reliable transformation from observed color magnitude diagrams to theoretical HR diagrams.
Color indices and bolometric corrections from ATLAS9 overshoot models (Kurucz, 1995a, priv. comm.) Color indices and bolometric corrections from ATLAS9 no-overshoot models (Castelli, 1997, priv. comm.) Color indices and bolometric corrections from ATLAS9 models for Teff>=9000K (Kurucz, 1993) Teff Effective temperature K logg Surface gravity [cm/s2] BC(K) Bolometric correction in Kmag mag BC(V) Bolometric correction in Vmag mag U-B U-B colour index mag B-V B-V colour index mag V-R V-R colour index mag V-I V-I colour index mag V-K V-K colour index mag J-H J-H colour index mag J-K J-K colour index mag K-L K-L colour index mag Color indices and bolometric corrections from NMARCS giant branch models of Plez, Brett and Nordlund (1992A&A...256..551P) Teff Effective temperature K logg Surface gravity [cm/s2] Mass Mass solMass BC(K) Bolometric correction in Kmag mag BC(V) Bolometric correction in Vmag mag B-V B-V colour index mag V-R V-R colour index mag V-I V-I colour index mag V-K V-K colour index mag J-H J-H colour index mag J-K J-K colour index mag K-L K-L colour index mag Color indices and bolometric corrections from NMARCS giant branch models of Plez (1995, priv. comm.). Color indices and bolometric corrections from NMARCS M dwarf models of Plez (1997, priv. comm.)* and Brett (1995A&A...295..736B and 1995A&AS..109..263B) Teff Effective temperature K Note *: Plez 1997 (priv. comm.) data in table6.dat --- logg Surface gravity [cm/s2] [Fe/H] Metallicity Sun BC(K) Bolometric correction in Kmag mag BC(V) Bolometric correction in Vmag mag B-V B-V colour index mag V-R V-R colour index mag V-I V-I colour index mag V-K V-K colour index mag J-H J-H colour index mag J-K J-K colour index mag K-L K-L colour index mag Patricia Bauer CDS 1998 Mar 05 Fiorella Castelli <castelli@astrts.oat.ts.astro.it> J_A+A_333_231.xml The overlapping open clusters NGC 1750 and NGC 1758. I. UBVRI-CCD photometry J/A+A/333/471 J/A+A/333/471 UBVRI photometry of NGC 1750 and NGC 1758 The overlapping open clusters NGC 1750 and NGC 1758. I. UBVRI-CCD photometry D Galadi-Enriquez C Jordi E Trullols I Ribas Astron. Astrophys. 333 471 1998 1998A&A...333..471G Clusters, open Photometry, UBVRI open clusters and associations: individual (NGC 1746, NGC 1750) stars: early-type The existence and relationship of the possible clusters NGC 1746, NGC 1750 and NGC 1758 has been a matter of discussion during the last decades. This star field is close to the galactic anticenter and lies in the direction of the Taurus dark cloud complex. As part of a comprehensive astrometric and photometric analysis of this zone, we present a brief historical introduction together with deep UBVRI-CCD photometry of the area. The presence of at least one cluster can be deduced from these data. This object has a position and apparent size compatible with those previously quoted for NGC 1750 and NGC 1758. It is not possible to distinguish the single or double nature of the cluster on the sole basis of our photometry and the spatial distribution of the stars. No photometric evidence was found for NGC 1746.
NGC 1746 C 0500+237 05 03.6 +23 49 NGC 1750 C 0500+235 05 03.9 +23 39 NGC 1758 C 0501+237 05 04.4 +23 47
UBVRI photometry for the 3224 program stars Seq Identification number=1 The stars numbers 1996, 1997, 2372, 3061 and 3162 were found to have anomalous photometric data and, thus, were eliminated from the catalogue. The number of entries is 3224, but the maximum identification number is 3229. --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag U-B U-B colour index mag e_U-B rms uncertainty on U-B mag V-R V-R colour index mag e_V-R rms uncertainty on V-R mag V-I V-I colour index mag e_V-I rms uncertainty on V-I mag xpos x coordinate number=2 There is a good alignment of +x coordinate with +alpha and of +y with +delta pix ypos y coordinate number=2 There is a good alignment of +x coordinate with +alpha and of +y with +delta pix Cross-identifications Seq Identification number --- SCM92b Straizys et al. (1992BaltA...1..125S) number --- CUF Cuffey (1937AnHar.105..403C) number --- PPM PPM (Cat. <I/146>) number --- BD BD (Cat. <I/122>) name --- HD HD (Cat. <III/135>) number --- TYC Tycho Catalogue (Cat. <I/239>) number --- Patricia Bauer CDS 1998 Feb 02 Carme Jordi <carme@pchpc7.am.ub.es> J_A+A_333_471.xml The Galactic globular cluster NGC 1851: its dynamical and evolutionary properties J/A+A/333/479 J/A+A/333/479 NGC 1851 dynamical and evolutionary properties The Galactic globular cluster NGC 1851: its dynamical and evolutionary properties I Saviane G Piotto F Fagotto S Zaggia M Capaccioli A Aparicio Astron. Astrophys. 333 479 1998 1998A&A...333..479S Clusters, globular Photometry, CCD globular clusters: individual (NGC 1851) Hertzsprung-Russell (HR diagram) stars: evolution stars: luminosity function, mass function stars: Population II We have completely mapped the Galactic globular cluster NGC 1851 with large-field, ground-based VI CCD photometry and pre-repair HST/WFPC1 data for the central region. The photometric data set has allowed a V vs. (V-I) colour-magnitude diagram for ~20500 stars to be constructed. From the apparent luminosity of the horizontal branch (HB) we derive a true distance modulus (m-M)_0_=15.44+/-0.20. An accurate inspection of the cluster's bright and blue objects confirms the presence of seven ``supra-HB'' stars, six of which are identified as evolved descendants from HB progenitors. The HB morphology is found to be clearly bimodal, showing both a red clump and a blue tail, which are not compatible with standard evolutionary models. Synthetic Hertzsprung-Russell (HR) diagrams demonstrate that the problem could be solved by assuming a bimodal efficiency of the mass loss along the red giant branch (RGB). With the aid of Kolmogorov-Smirnov statistics we find evidence that the radial distribution of the blue HB stars is different from that of the red HB and supgiant branch (SGB) stars. We give the first measurement of the mean absolute I magnitude for 22 known RR Lyr variables (<M_I_(RR)>=0.12+/-0.20mag at a metallicity [Fe/H]=-1.28). The mean absolute V magnitude is <M_V_(RR)>=0.58+/-0.20mag, and we confirm that these stars are brighter than those of the zero-age HB (ZAHB). Moreover, we found seven new RR Lyr candidates (six ab type and one c type). With these additional variables the ratio of the two types is now N_c_/N_ab_=0.38. From a sample of 25 globular clusters a new calibration for {DELTA} V_bump_^HB^ as a function of cluster metallicity is derived. NGC 1851 follows this general trend fairly well. From a comparison with the theoretical models, we also find some evidence for an age-metallicity relation among globular clusters. We identify 13 blue straggler stars, which do not show any sign of variability. The blue stragglers are less concentrated than the subgiant branch stars with similar magnitudes for r>80arcsec. Finally, a radial dependence of the luminosity function, a sign of mass segregation, is found. Transforming the luminosity function into a mass function (MF) and correcting for mass segregation by means of multi-mass King-Michie models, we find a global MF exponent x_0_=0.2+/-0.3.
NGC 1851 C 0512-400 05 14 06.3 -40 02 50
appen.ps PostScript version of Appendix appen.tex LaTeX version of Appendix cback.ps V-v_norm_ versus V-I diagram field1ms.ps Completeness as a function of magnitude and radius for the central field xfig.ps Plot of the photometric zero-point differences Patricia Bauer CDS 1998 Feb 16 Ivo Saviane <saviane@astrpd.pd.astro.it> J_A+A_333_479.xml A lithium-survey for pre-main sequence stars in the upper Scorpius OB association J/A+A/333/619 J/A+A/333/619 Upper Scorpius OB association Lithium survey A lithium-survey for pre-main sequence stars in the upper Scorpius OB association T Preibisch E Guenther H Zinnecker M Sterzik S Frink S Roeser Astron. Astrophys. 333 619 1998 1998A&A...333..619P Associations, stellar Equivalent widths Proper motions Stars, pre-main sequence open clusters and associations: individual (Scorpius, Centarus) stars: kinematics stars: pre-main sequence surveys X-rays: stars We present the results of an intermediate resolution spectroscopic survey for pre-main sequence (PMS) stars in the Upper Scorpius OB association. In a 160 square-degree area we were able to identify 39 new PMS stars by follow up observations of X-ray selected stars with the multi object spectrograph FLAIR at the UK Schmidt Telescope. We also investigated the completeness of our X-ray selected sample by observing more than 100 stars that were not detected as X-ray sources, but have proper motions indicating membership to Upper Sco. While the new X-ray selected PMS stars with known proper motions have kinematics consistent with membership, none of the X-ray quiet proper motion candidates is a PMS star. We conclude that our X-ray selected sample of PMS stars seems to be rather complete. For stars in the magnitude interval 11.5<~B<~13.5 we derive a conservative lower limit of 75% completeness.
Results for the X-ray selected PMS candidates GSC GSC (Cat. <I/220>) number --- Index See Note number=1 empty: X-ray source detected in the ROSAT All Sky Survey P: X-ray source detected in pointed ROSAT observation only --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Bmag B magnitude from GSC (Cat. <I/220>) mag CR ROSAT count rate ct/s u_CR Uncertainty/upper limit note number=2 "<": Upper limit to the line width ":": Uncertainty exceeding 15% --- W(Li) Li line equivalent width 0.1nm u_W(Li) Uncertainty/upper limit note number=2 "<": Upper limit to the line width ":": Uncertainty exceeding 15% --- W(Ha) H{alpha} line equivalent width 0.1nm SpType Spectral type --- u_SpType Uncertainty flag on SpType --- Type See Note number=3 Classification of the objects PMS: pre-main sequence star YC: non-PMS star with a Lithium line as typical for stars in the young clusters mentioned in Section 4 F: non-PMS star with a very weak lithium line (probably active field star) --- pmRA Proper motion in right ascension *cos(delta) mas/yr pmDE Proper motion in declination mas/yr Results for the proper motion selected PMS candidates GSC GSC (Cat. <I/220>) number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Bmag B magnitude from GSC mag u_Bmag Uncertainty/upper limit note number=1 <": Upper limit to the line width ":": Uncertainty exceeding 15% --- W(Li) Li line equivalent width 0.1nm u_W(Li) Uncertainty/upper limit note number=1 <": Upper limit to the line width ":": Uncertainty exceeding 15% --- W(Ha) H{alpha} line equivalent width 0.1nm SpType Spectral type --- u_SpType Uncertainty flag on SpType --- Type See Note number=2 Classification of the objects YC: non-PMS star with a Lithium line as typical for stars in the young clusters mentioned in Section 4 F: non-PMS star with a very weak lithium line (probably active field star) --- pmRA Proper motion in right ascension *cos(delta) mas/yr pmDE Proper motion in declination mas/yr Patricia Bauer CDS 1998 Feb 13 Thomas Preibisch <preib@astro.uni-wuerzburg.de> J_A+A_333_619.xml Spectroscopic observations of D-type symbiotic stars J/A+A/333/658 J/A+A/333/658 D-type symbiotic stars emission line fluxes Spectroscopic observations of D-type symbiotic stars C B Pereira S J C Landaberry S Junqueira Astron. Astrophys. 333 658 1998 1998A&A...333..658P III/174 : Atlas of line profiles of symbiotic stars (VanWinckel+, 1994) Binaries, spectroscopic Spectroscopy stars: abundances stars: symbiotic Observations of five D-type symbiotics are presented: three oxygen Mira (He2-38, H2-38 and H1-36) and two carbon Mira symbiotics (AS 210 and SS 38). The observations in the spectral range between 3200{AA} and 7400{AA} show the presence of several emission lines in various states of excitation. A line list is provided with their suggested identifications. Several parameters were derived for each object: interstellar reddening as determined from Balmer decrement and He II lines, temperature and electronic density, abundance ratios of Ne/O, Ar/O, Fe/Ne, N/O and He/H. We found nitrogen enrichment while for the other elements their abundances are compatible with solar, except iron which is depleted. We did not detect significant changes in the line and in the continuos spectra of the stars analyzed here, except for He2-38, which increased its degree of excitation compared to Allen's (1984PASAu...5..562N) catalogue.
Hen 2-38 V366 Car PK 280-02 1 09 54 43.2 -57 18 53 AS 210 Hen 3-1265 PK 355+11 1 16 51 20.4 -26 00 27 PN H 2-38 PK 002-03 4 Hen 2-343 18 06 01.0 -28 17 06 PN H 1-36 PK 353-04 1 Hen 2-289 17 49 48.1 -37 01 28 SS 38 06 21 04.4 +22 10 12
Observed emission line fluxes relative to H-{beta} = 100 lambda Wavelength 0.1nm Ion Ion --- n_Ion Note on Ion number=1 O VI Raman scattered w1 : present in NGC 7027 , Wyse (1942ApJ....95..356W) w2 : present in NGC 7027 , Wyse (1942ApJ....95..356W) w3 : present in NGC 6741 , Wyse (1942ApJ....95..356W) --- He2-38 Relative line fluxes of He2-38 (H{beta}=100) --- AS210 Relative line fluxes of AS 210 (H{beta}=100) --- H2-38 Relative line fluxes of H2-38 (H{beta}=100) --- H1-36 Relative line fluxes of H1-36 (H{beta}=100) --- SS38 Relative line fluxes of SS 38 (H{beta}=100) --- table7.tex LaTeX version of table2 Patricia Bauer CDS 1998 Jan 30 Claudio Pereira <claudio@balmer.physics.utep.edu> J_A+A_333_658.xml Evolution of mass segregation in open clusters: some observational evidences J/A+A/333/897 J/A+A/333/897 Mass segregation in open clusters Evolution of mass segregation in open clusters: some observational evidences D Raboud J -C Mermilliod Astron. Astrophys. 333 897 1998 1998A&A...333..897R J/A+A/325/167 : Geneva photometry in NGC 6231 (Raboud+ 1997) Clusters, open Photometry Stars, distances Stars, masses open clusters and associations: general open clusters and associations: individual (Praesepe, NGC 6231) stars: formation On the basis of the best available member list and duplicity information, we have studied the radial structure of Praesepe and of the very young open cluster NGC 6231. We have found mass segregation among the cluster members and between binaries and single stars, which is explained by the greater average mass of the multiple systems. However, the degree of mass segregation for stars between 1.5 and 2.3M_{sun}_ is less pronounced in Praesepe than in the Pleiades. Furthermore, mass segregation is already present in the very young open cluster NGC 6231 although this cluster is likely still not dynamically relaxed. We discuss the implications of these results and propose a qualitative scenario for the evolution of mass segregation in open clusters. In Praesepe the mass function of single stars and primaries appears to be significantly different, like in the Pleiades. We observe an absence of ellipticity of the outer part of Praesepe.
Praesepe NGC 2632 M 44 08 40.4 +19 40 NGC 6231 16 54.2 -41 48
Member stars in Praesepe KW Star identification (Cl* NGC 2632 KW NNN in Simbad database) --- Vmag V magnitude mag B-V B-V colour index mag xpos x coordinate number=1 Origin (1950.0), RA = 08 37 32 ; DE = +19 48.8 y increasing to North , x to East arcmin ypos y coordinate number=1 Origin (1950.0), RA = 08 37 32 ; DE = +19 48.8 y increasing to North , x to East arcmin Dist Distance from the cluster center arcmin Mult Multiplicity status --- Rem Remarks --- MassTot Total mass solMass MassA Component A mass solMass MassB Component B mass solMass MassC Component C mass solMass Member stars in NGC 6231 NGC6231 Star identification (NGC 6231 NNN in Simbad database) --- Vmag V magnitude mag col Colour ((B-V)J, (B_V)G or b-y) number=1 The colour is (B-V)_Johnson if the photometry used (phot column) is UBV, (B-V)_Geneva if the photometry used is Gen and (b-y) if the photometry used is uvby. mag phot Photometry used (Gen, UBV or uvby) --- xpos x coordinate number=2 Origin (1950.0) RA = 16 50 41 ; DE =-41 44.9 y increasing to North , x to East arcmin ypos y coordinate number=2 Origin (1950.0) RA = 16 50 41 ; DE =-41 44.9 y increasing to North , x to East arcmin Dist Distance from the cluster center arcmin Mult Multiplicity status --- Rem Remarks --- MassTot Total mass solMass MassA Component A mass solMass MassB Component B mass solMass Raboud Geneva Observatory 1998 Feb 20 Didier Raboud <Didier.Raboud@obs.unige.ch> J_A+A_333_897.xml The possible effects of an unusual resonance in very long period Cepheids J/A+A/333/L35 J/A+A/333/L35 Magellanic Clouds Cepheids Fourier decomposition The possible effects of an unusual resonance in very long period Cepheids E Antonello Astron. Astrophys. 333, L35 ??? ??? 1998 1998A&A...333L..35A Magellanic Clouds Radial velocities Stars, variable Cepheids Magellanic Clouds stars: oscillations The radial velocity and light curves of 24 Cepheids in the Magellanic Clouds, with period in the range 30-134d, were Fourier decomposed with the aim of detecting resonance effects between pulsation modes. The Tables contain the list of stars, the details of the analysis and the Fourier parameters.
List of 24 Cepheids in the Magellanic Clouds, with period in the range 30-134 d, whose radial velocity and light curves were Fourier decomposed HV Star name (Harvard Variable number) SV* HV NNNNN in Simbad Database --- n_HV L: LMC; S: SMC --- LCPer Light curves: period d n_LC Light curves: data points --- r_LC Light curves: references of data sources number=1 1 = Gascoigne & Kron (1965MNRAS.130..333G) 2 = Madore (1975ApJS...29..219M) 3 = VanGenderen (1977A&A....54..737V, 1983A&AS...52..423V) 4 = Martin & Warren (1979SAAOC...1...98M) 5 = Eggen (1977ApJS...34....1E) 6 = Freedman et al. (1985ApJS...59..311F) 7 = Imbert et al. (1985A&AS...61..259I) 8 = Imbert et al. (1989A&AS...81..339I) 9 = Imbert (1994A&AS..105....1I) 10 = Sebo & Wood (1995ApJ...449..164S, Cat. <J/ApJ/449/164>) --- LCorder Light curves: order of Fourier fit --- e_LC Light curves: standard deviation of the fit mag RVCPer Radial velocity curves: period (days) d n_RVC Radial velocity curves: data points --- r_RVC Radial velocity curves: references of data sources number=1 1 = Gascoigne & Kron (1965MNRAS.130..333G) 2 = Madore (1975ApJS...29..219M) 3 = VanGenderen (1977A&A....54..737V, 1983A&AS...52..423V) 4 = Martin & Warren (1979SAAOC...1...98M) 5 = Eggen (1977ApJS...34....1E) 6 = Freedman et al. (1985ApJS...59..311F) 7 = Imbert et al. (1985A&AS...61..259I) 8 = Imbert et al. (1989A&AS...81..339I) 9 = Imbert (1994A&AS..105....1I) 10 = Sebo & Wood (1995ApJ...449..164S, Cat. <J/ApJ/449/164>) --- RVCorder Radial velocity curves: order of Fourier fit --- e_RVC Radial velocity curves: standard deviation of the fit km/s Phase differences and amplitude ratios of the light curves of 20 Cepheids Phase differences and amplitude ratios of the radial velocity curves of 17 Cepheids HV Star Name (Harvard Variable number) SV* HV NNNNN in Simbad Database --- phi21 Phase difference phi_21 (rad) rad R21 Amplitude ratio R_21 --- phi31 Phase difference phi_31 rad R31 Amplitude ratio R_31 --- phi41 Phase difference phi_41 rad R41 Amplitude ratio R_41 --- phi51 Phase difference phi_51 rad R51 Amplitude ratio R_51 --- phi61 Phase difference phi_61 rad R61 Amplitude ratio R_61 --- phi71 Phase difference phi_71 rad R71 Amplitude ratio R_71 --- phi81 Phase difference phi_81 rad R81 Amplitude ratio R_81 --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Mar 17 Elio Antonello <elio@merate.mi.astro.it> J_A+A_333_L35.xml Infrared carbon stars: new identifications and their space distribution in the Galaxy J/A+A/334/609 J/A+A/334/609 Carbon stars IR photometry Infrared carbon stars: new identifications and their space distribution in the Galaxy F Guglielmo T Le Bertre N Epchtein Astron. Astrophys. 334 609 1998 1998A&A...334..609G II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) III/197 : IRAS Low Resolution Spectra (IRAS team, 1987) Cross identifications Photometry, infrared Stars, carbon circumstellar matter Galaxy: stellar content infrared: stars stars: AGB and post-AGB stars: carbon stars: late-type We present JHKL photometry of a sample of 150 IRAS stars in the third and fourth galactic quadrant with |b|<2{deg} selected according to their IRAS colour (0.160<=[12-25]<=1.156). We identify 27 carbon star candidates using the [12-25] vs. K-L two-colour diagram method. Among them, 10 are listed in the Stephenson's catalogue of carbon stars and 17 are new infrared carbon stars (IRCS) candidates. Their distances are found to be larger than 3kpc. These data are combined with previous data to study the space distribution of IRCS. The number density seems to be independent of the galactocentric distance (R) toward the Galactic Center and to decrease exponentially toward the anticenter. At the present stage, it is not possible to disentangle effects such as incompleteness of the sample, different space distribution law and dependence of the luminosity on metallicity. In particular, we suggest that the apparent scarcity of IRCS in the central direction of the Galaxy (R<5kpc) might be due to a selection effect. From the available data, we have found no IRCS within 1kpc of the Galactic Center.
Observations IRAS IRAS Name --- Kmag K magnitude mag J-K J-K colour index mag H-K H-K colour index mag K-L K-L colour index mag [12-25] Infrared [12-25] colour index mag [25-60] Infrared [25-60] colour index mag IRASClass IRAS Low Resolution Spectrometer class (Olnon et al., 1986A&AS...65..607O) --- ValClass Valinhos class (Epchtein et al. 1987A&AS...71...39E) --- VeenClass van der Veen & Habing class (1988A&A...194..125V) --- Ident Identifications indicated in table4.dat number=1 C: Identification in CGCS (Cat. <III/156>) S: Identification in GCSS (Cat. <III/60>) I: No identifications in CGCS or GCSS catalogues --- Identifications IRAS IRAS name --- GCVS General Catalogue of Variable Stars (Kholopov et al., 1985, Cat. <II/139>) --- TMSS Two Micron Sky Survey (Cat. <II/2>) --- RAFGL Revised Air Force Geophysics Laboratory Infrared Sky Survey (Cat. <II/94>) --- CGCS Stephenson 1989, General Catalog of Cool Galactic Carbon Stars (Cat. <III/156>) or Stephenson 1976, Cat. <III/60> for number preceded by an S --- Other Other names number=1 CNS: Catalog of nearby stars (Gliese 1969), Cat. <V/35> DO: Dearborn Observatory Catalogue of Faint Red Stars (Lee et al. 1943, 1944, 1947) Cat. <II/68> EIC: Equatorial Infrared Catalogue (Sweeney et al. 1978) Cat. <II/161> SAO: Smithsonian Astrophysical Observatory Star Catalog (Smithsonian Institution 1966) See Cat. <I/131> NCSV: New Catalogue of Suspected Variable Stars (Kukarkin et al. 1981) Cat. <II/140> --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1998 Feb 20 Thibaut Le Bertre <LEBERTRE@mesioa.obspm.fr> J_A+A_334_609.xml The active RS Canum Venaticorum binary II Pegasi. I. Stellar and orbital parameters. J/A+A/334/863 J/A+A/334/863 II Peg radial velocities The active RS Canum Venaticorum binary II Pegasi. I. Stellar and orbital parameters. S V Berdyugina S Jankov I Ilyin I Tuominen F C Fekel Astron. Astrophys. 334 863 1998 1998A&A...334..863B Binaries, spectroscopic Radial velocities binaries: spectroscopic stars: abundances stars: activity stars: fundamental parameters stars: individual (II Peg) A detailed model atmosphere analysis of high-resolution and high S/N CCD spectra of IIPeg has yielded for the first time a self-consistent set of fundamental parameters of the primary component: T_eff_=4600K, logg=3.2, [M/H]=-0.4, {xi}_t_=2.0km/s. In addition, 121 new high quality radial velocity measurements allowed us to determine improved orbital parameters, resulting in a new orbital ephemeris of T_conj_=2449582.9268+6.724333E. The position of the primary of II Peg in the HR diagram with the new parameters corresponds to a K2 IV star with mass =~0.8M_{sun}_. The evolved character of the star is confirmed by the C/N ratio, which is reduced significantly relative to the solar value. The unspotted V magnitude of the star of 6.9mag is estimated from the observed variations of the TiO bands and quasi-simultaneous photometry. The blend of LiI 6707{AA} is suspected to vary in equivalent width due to spot modulation. The lithium abundance for the unspotted star, Li/H=1.0+/-0.1, is found to be consistent with other post-main sequence chromospherically active stars. Combining all parameters, the radius R=~3.4R_{sun}_ and the inclination i=~60{deg} of the primary are estimated with the assumption that its rotational axis is perpendicular to the orbital plane. The secondary is probably a M0-M3 V star with a mass of about 0.4M_{sun}_.
II Peg HD 224085 23 55 01.8 +28 37 59
Radial velocity data HJD Heliocentric Julian date d RV Radial velocity km/s r_RV Reference for radial velocity number=1 1: Sanford (1921ApJ....53..201S) 2: Halliday (1952JRASC..46..103H) 3: Heard (1956PDDO....2..105H) 4: Rucinski (1977PASP...89..280R) 5: Vogt (1981ApJ...247..975V) 6: SOFIN echelle spectrograph (Nordic Optical Telescope, Roque de los Muchocohs Observatory 7: Crimea Astrophysical Observatory 8: McDonald Observatory 9: Kitt Peak National Observatory --- Patricia Bauer CDS 1998 May 19 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+A_334_863.xml New identifications for blue objects towards the Galactic center: post-AGB stars, Be/disk stars, and others J/A+A/334/987 J/A+A/334/987 6 blue objects spectral data New identifications for blue objects towards the Galactic center: post-AGB stars, Be/disk stars, and others K A Venn S J Smartt D J Lennon P L Dufton Astron. Astrophys. 334 987 1998 1998A&A...334..987V VI/72 : Atomic Transition Probabilities, Sc-Ni (NIST 1993) Blue objects Spectroscopy Stars, early-type galaxies: fundamental parameters Galaxy: center stars: abundances stars: AGB and post-AGB stars: emission-line, Be supergiants supergiants As part of a programme to investigate spatial variations in the Galactic chemical composition, we have been searching for normal B-type stars and A-type supergiants near the Galactic center. During this search we have found eleven peculiar stars, and in some cases performed detailed abundance analyses of them which suggest that they may be at a post-AGB evolutionary stage. The A-type post-AGB candidates show [Fe/H]=-1.0 to -2.0, and [O/Fe]~+1.4, typical of the post-AGB abundance patterns discussed in the literature. One star, LS 3591 (=SAO 243756), has also been examined recently by Oudmaijer (1996A&A...306..823O); its spectrum appears to be changing very rapidly, which may indicate erratic mass loss or the incipient formation of a planetary nebula. A B-type post-AGB candidate, LS 4950, has a similar spectrum to a well studied post-AGB star, LSIV -12 111. However, an examination of the line strengths and elemental abundances of LS 4950 show that it is peculiar for both a PopulationII, post-AGB, B-type star and for a normal, PopulationI, B-type supergiant. Two other B-type stars, LS 4825 and LS 5112, are either post-AGB stars near the Galactic center or normal B-type supergiants lying well beyond the Galactic center. In addition, several Be-type stars have been newly (or more clearly) identified from our spectra.
LS 3591 16 25 02.5 -60 03 32 LS 3593 16 24 39.3 -54 38 08 LS 4950 18 21 47.0 -29 45 07 LS 4039 17 17 07.4 -24 45 40 LS 4825 18 16 00.4 -30 45 46 LS 5112 18 40 48.4 -17 04 36
*Spectral line data for two post-AGB A-type stars Ion Ion --- lambda Wavelength 0.1nm RMT Multiplet number --- chi Excitation potential eV loggf log of oscillator strength --- EWLS3591 Equivalent width for the star LS 3591 0.1nm u_EWLS3591 Uncertainty flag on EWLS3591 --- EWLS3593 Equivalent width for the star LS 3593 0.1nm r_loggf Reference for the oscillator strength number=1 References for the atomic data. fmw = Fuhr, Martin & Wiese 1988, Cat. <VI/72>, J. Phys. Chem. Ref. Data 17, Suppl.4. nk = Kurucz 1990, Trans IAV B, 20, 168 (magnetic tape) ob = O'Brien et al. 1991, J. Opt. Soc. Am. B, 8, 1185 op = Opacity Project (O I, Hibbert et al. 1991, J. Phys B, 24, 3943) zhu = Zhu et al. 1989, Phys Rev A., 40, 3721 wm = Wiese & Martin 1980, NSRDS-NBS 68 wsm = Wiese, Smith, & Martin 1969, NSRDS-NBS 22 sl = Sigut & Landstreet, 1990MNRAS.247..611S --- *Spectral line data for four B-type stars towards the Galactic Center Ion Ion number=1 All atomic data has been taken from the compilation by S. Jeffrey 1991 Newsletter on the Analysis of Astronomical Spectra, No. 16, p. 17. --- lambda Wavelength 0.1nm --- Separation comma --- lambda2 Second wavelength number=2 Where two lines are listed together, they represent an unresolved blend (only blends of the same species are included). 0.1nm EWLS4950 Equivalent width for the star LS 4950 0.1nm EWLS4039 Equivalent width for the star LS 4039 0.1nm EWLS4825 Equivalent width for the star LS 4825 0.1nm EWLS5112 Equivalent width for the star LS 5112 0.1nm appen.tex LaTeX version of the tables appen.ps PostScript version of the tables Patricia Bauer CDS 1998 Mar 23 Kim A Venn <venn@clare.physics.macalester.edu> J_A+A_334_987.xml The rotational velocity of low-mass stars in the Pleiades cluster J/A+A/335/183 J/A+A/335/183 Pleiades low-mass stars rotational velocities The rotational velocity of low-mass stars in the Pleiades cluster D Queloz S Allain J -C Mermilliod J Bouvier M Mayor Astron. Astrophys. 335 183 1998 1998A&A...335..183Q I/90 : Positions of 502 Stars in Pleiades Region (Eichhorn+ 1970) J/A+A/320/74 : Radial velocities of Pleiades members (Mermilliod+ 1997) J/ApJS/85/315 : F, G and K dwarf stars of the Pleiades (Soderblom+ 1993) Clusters, open Radial velocities Rotaional velocities Stars, pre-main sequence Stars, white dwarf open clusters and associations: individual (Pleiades) stars: activity stars: evolution stars: pre-main sequence We present new vsini measurements for 235 low-mass stars in the Pleiades. The differential rotational broadening has been resolved for all the stars in our sample. These results, combined with previously published measurements, provide a complete and unbiased rotation data set for stars in the mass range from 0.6 to 1.2M_{sun}_. Applying a numerical inversion technique on the vsini distributions, we derive the distributions of equatorial velocities for low-mass Pleiades members. We find that half of the Pleiades dwarfs with a mass between 0.6 to 1M_{sun}_ have rotation rates lower than 10km/s.
*CORAVEL and ELODIE vsini measurements of Pleiades stars from the Hertzsprung (1947AnLei..19a...1H, see Cat. <I/90>) and Soderblom (1993, Cat. <J/ApJS/85/315>) samples. Star Star number (Cl Melotte 22 NNN in Simbad) --- m_Star Multiplicity index on Star for each component of a SB2 system --- n_Star Note on Star number=1 +: Binary systems with rotations synchronized to the orbital motion. *: Suspected long period double line spectroscopic binary (unresolved) --- B-V0 B-V_0_ colour index mag l_vsiniC Limit flag on vsiniC --- vsiniC CORAVEL rotational velocity km/s e_vsiniC rms uncertainty on vsiniC km/s n_vsiniC Note number=2 n: Stars detected as "no dip" by CORAVEL are unresolved very fast rotators (vsini>60km/s) S: SB2, double line spectroscopic binary where the two components are unresolved --- vsiniE ELODIE rotational velocity km/s e_vsiniE rms uncertainty on vsiniE km/s CORAVEL vsini measurement of stars located in the corona of the Pleiades and recently selected by Rosvick et al. (1992A&A...255..130R) and by Mermilliod et al. (1997, Cat. <J/A+A/320/74>) as cluster members. Star Star name number=1 Pels NNN = CL* MELOTTE 22 PELS NNNN in Simbad Ia 317 = Cl* Melotte 22 AK I-1-317 in Simbad Ib NNN = Cl* Melotte 22 AK I-2-NNN in Simbad AAA NNN = Cl* Melotte 22 AK AAA-NNN in Simbad SNNNx = Cl* Melotte 22 TRU SNNN x in Simbad SNN = Cl* Melotte 22 TRU SNN in Simbad --- n_Star Note on Pels 39 number=2 *: Pels 39 lies slightly above the main sequence but doesn't show any hint of binarity with radial velocities. However, its very small vsini value is an indication that this star could be a non-member. --- mag (B-V)0 mag l_vsini Limit flag on vsini --- vsini Rotational velocity km/s e_vsini rms uncertainty on vsini km/s n_vsini Note on vsini number=3 n: Stars detected as "no dip" by CORAVEL are unresolved very fast rotators (vsini>60km/s) S: SB2, double line spectroscopic binary where the two components are unresolved --- ELODIE vsini and radial velocity measurements of new members of the Pleiades corona. Pels Star name (CL* MELOTTE 22 PELS NNNN) in Simbad --- (B-V)0 (B-V)_0_ colour index mag vsini Rotational velocity km/s e_vsini rms uncertainty on vsini km/s RV Radial velocity km/s u_RV Uncertainty flag on RV --- O-C Velocity difference with the mean velocity of the cluster corrected from the projection effect number=1 Note that, in order to use the convergent point measured by Rosvick et al. (1992A&A...255..130R) to compute the (O-C), the ELODIE measurements have been converted into the CORAVEL zero point reference frame. The following velocity offset has been used: V_E_-V_C_ = 0.48 - 1.45(B-V) + 0.53(B-V)^2^ (Udry et al., 1998, in prep.). km/s tables.tex LaTex version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Jun 18 Jean-Claude Mermilliod <Jean-Claude.Mermilliod@obs.unige.ch> J_A+A_335_183.xml Identification of soft high galactic latitude RASS X-ray sources. I. A complete count-rate limited sample. J/A+A/335/467 J/A+A/335/467 High galactic latitude RASS X-ray sources Identification of soft high galactic latitude RASS X-ray sources. I. A complete count-rate limited sample. H -C Thomas K Beuermann K Reinsch A D Schwope J Truemper W Voges Astron. Astrophys. 335 467 1998 1998A&A...335..467T IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) J/MNRAS/274/1165 : The 2RE Source Catalogue (Pye+ 1995) J/MNRAS/274/1194 : Optical Identifications of ROSAT EUV Sources (Mason+ 1995) Cross identifications X-ray sources galaxies: Seyfert novae, cataclysmic variables stars: coronae white dwarfs X-rays: galaxies X-rays: stars We present a summary of spectroscopic identifications for a complete sample of bright soft high galactic latitude X-ray sources drawn from the ROSAT All-Sky Survey which have PSPC count-rates CR>0.5cts/s and hardness ratios HR1<0. Of a total of 397 sources, 270 had catalogued counterparts although most of these were not previously known as X-ray sources; of the remaining 127 sources neither X-ray nor optical properties were previously known. Of the whole sample of very soft X-ray sources 155 were also discovered by the Wide-Field-Camera on board ROSAT. We present spectroscopic identifications of 108 sources and other identifications for further 18 sources; 1 source remains unidentified so far. In practically all cases a unique optical counterpart exists facilitating identification. The largest source classes are AGN, magnetic cataclysmic variables, and hot white dwarfs.
Summary of the optical identification program for previously known sources in our sample. 1RXS 1RXS designation --- n_1RXS Note on the object number=1 1RXS J035025.0+171455 (V471 Tau): HR1=-0.7, white dwarf companion (Werner & Rauch, 1997A&A...324L..25W and references therein) 1RXS J041521.5-073843 (40 Eri): HR1=-0.3, white dwarf companion 1RXS J132511.6-110932 (Spica): HR1=-0.9, coronal emission (Cassinelli et al., 1994ApJ...421..705C) --- Name Name of the optical counterpart --- SpType Spectral type of the counterpart --- Sep Separation between optical and X-ray positions arcsec Sep(r90) Separation between optical and X-ray positions in units of the 90% confidence radii --- Summary of the optical identification program for new sources in our sample. 1RXS 1RXS designation --- RAh Optical counterpart right ascension (2000) h RAm Optical counterpart right ascension (2000) min RAs Optical counterpart right ascension (2000) s DE- Declination sign --- DEd Optical counterpart declination (2000) deg DEm Optical counterpart declination (2000) arcmin DEs Optical counterpart declination (2000) arcsec Sep Separation between optical and X-ray positions in arcsec arcsec Sep(r90) Separation between optical and X-ray positions in units of the 90% confidence radii --- CR RASS BSC PSPC count-rate ct/s e_CR rms uncertainty on CR 10-2ct/s HR1 Hardness ratio HR1 --- e_HR1 rms uncertainty on HR1 10-2 Class Classification of the optical counterpart --- Type Type of the optical counterpart --- z Redshift if extragalactic --- u_z Uncertainty flag on z --- Vmag V magnitude mag Note Notes number=1 1: spectroscopic identification, this work 2: WFC identification (Pye et al., 1995, Cat. <J/MNRAS/274/1165>, Mason et al., 1995, Cat. <J/MNRAS/274/1194>) 3: Hamburg/RASS identification (Bade et al., 1998A&AS..127..145B) 4: Grupe et al., 1998A&A...330...25G 5: inferred identification from the Digitized Sky Survey (see Sect. 3.2) 6: radio source (see Sect. 3.2) 7: blank field 8: Remarks to individual sources in notes.dat file --- Individual notes 1RXS 1RXS designation --- Note Text of the note --- Patricia Bauer CDS 1998 Nov 27 Hans-Christoph Thomas <hcthomas@MPA-Garching.MPG.DE> J_A+A_335_467.xml Investigation of the variability of bright Be stars using Hipparcos photometry J/A+A/335/565 J/A+A/335/565 Be stars variability Investigation of the variability of bright Be stars using Hipparcos photometry A -M Hubert M Floquet Astron. Astrophys. 335 565 1998 1998A&A...335..565H I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Stars, Be Stars, variable stars: emission-line, Be stars: oscillations stars: statistics stars: variables: other The high accuracy and the homogeneity of Hipparcos data for bright stars have allowed us to quantify the degree of variability of Be stars. This degree has been found to be highly dependent on the temperature of the star. Rapid variability is the main feature of the 86% of early Be and less than 20% of late Be stars taking into account the limit of detection considered. In addition to Be stars reported in the Hipparcos catalogue (ESA 1997, Cat. <I/239>) as short-period variables, we have been able to enlarge the number of detections as well as to confirm periods previously determined. Be stars that show larger amplitude rapid variations are proposed as candidates for a search of multiperiodicity i.e. as non-radial pulsators. We have also searched for the presence of outbursts and fading events in the Hipparcos data. Outbursts have been frequently and preferentially detected in early Be stars with rather low to moderate v sini while fading events seem to be more conspicuous in stars with higher v sini. Mid-term and long-term variations have also been investigated. Several stars have shown some evidence of temporary quasi-periodic oscillations ranging between 10 and 200 days. Finally information concerning long-term variations is reported. Cycles shorter than or equal to the Hipparcos mission have mainly been detected in stars earlier than B6. Long-term time scales of late Be stars are confirmed to be longer by far.
Short-term variability of Be stars using FT+CLEAN Short-term periodicity of Be stars given by Hipparcos catalogue (Cat. <I/239>) HD HD (Cat. <III/135>) number --- Name Star's name --- Vmag V magnitude mag n_Vmag Note on Vmag number=1 *: The V magnitude given by Hipparcos is the magnitude of the photocenter of this multiple system --- SpType Spectral type of the star number=2 Sources of the spectral classification are Jaschek et al. (1980A&AS...42..103J), Slettebak (1982ApJS...50...55S) and Zorec & Briot (1991A&A...245..150Z). --- Var Long-term variation --- l_Per Limit flag on Per --- Per Period of short-term variations d --- Dash --- Per2 Second period of short-term variations d u_Per Uncertainty flag on Per --- n_Per DW when light curve presents a double wave --- Rem Remarks number=3 References: 1- Bozic et al., 1995, Cat. <J/A+A/304/235> 2- Percy et al., 1994PASP..106..131P 3- Dachs & Lemmer 1991, in "Rapid Variability of OB stars: Nature and Diagnostic Value", Garching, p 103 4- Stefl & Balona, 1996, Cat. <J/A+A/309/787> 5- Balona et al., 1992A&AS...92..533B 6- Yang et al., 1990ApJS...74..595Y 7- Kaye & Gies, 1997ApJ...482.1028K 8- Balona, 1995MNRAS.277.1547B 9- Barrera et al., 1991Ap&SS.185...79B 10- Cuypers et al., 1989A&AS...81..151C 11- Stagg et al., 1988MNRAS.234.1021S 12- Bossi et al., 1989IBVS.3348....1B 13- Balona et al., 1992A&AS...92..533B 14- Stefl et al., 1995, Cat. <J/A+A/294/135> --- Patricia Bauer CDS 1998 Mar 31 Michele Floquet <Michele.Floquet@obspm.fr> J_A+A_335_565.xml Very low mass stars: non-linearity of the limb-darkening laws J/A+A/335/647 J/A+A/335/647 Limb-darkening coefficients for ubvyUBVRIJHK Very low mass stars: non-linearity of the limb-darkening laws A Claret Astron. Astrophys. 335 647 1998 1998A&A...335..647C J/A+AS/109/441 : Stellar models until He burning - I. (Claret, 1995) J/A+AS/114/549 : Stellar models until He burning - II. (Claret+, 1995) J/A+AS/125/439 : Stellar models until He burning - III. (Claret+, 1997) J/A+AS/110/329 : LTE model atmospheres coeff. (Diaz-cordoves+, 1995) J/A+AS/114/247 : Limb-darkening coefficients for RIJHK (Claret+, 1995) Binaries, eclipsing Models, evolutionary binaries: eclipsing stars: atmospheres stars: low-mass, brown dwarfs Linear and non-linear limb-darkening coefficients for the photometric bands u v b y U B V R I J H K are computed for very low effective temperatures stars. The atmosphere models used (PHOENIX-NextGen) do not include the effects of dust formation and dust opacities. These calculations are presented for the first time . The calculations extend the range of effective temperatures (2000K-50000K) covered by our previous papers. These data are important in order to deal with stars in the lower part of Main-Sequence like M or brown dwarfs. The non-linear behavior of the limb-darkening laws, particularly in this effective temperature range, is emphasized and we urge users to take it into account.
Linear (u) limb-darkening coefficients Quadratic (a, b) limb-darkening coefficients Square root (c, d) limb-darkening coefficients Coeff Limb-darkening coefficient number=1 u for linear, (a, b) for quadratic and (c, d) for square root limb-darkening coefficients --- logg Surface gravity cm/s2 Teff Effective temperature K u Limb-darkening coefficient (Filter u) --- v Limb-darkening coefficient (Filter v) --- b Limb-darkening coefficient (Filter b) --- y Limb-darkening coefficient (Filter y) --- U Limb-darkening coefficient (Filter U) --- B Limb-darkening coefficient (Filter B) --- V Limb-darkening coefficient (Filter V) --- R Limb-darkening coefficient (Filter R) --- I Limb-darkening coefficient (Filter I) --- J Limb-darkening coefficient (Filter J) --- H Limb-darkening coefficient (Filter H) --- K Limb-darkening coefficient (Filter K) --- Patricia Bauer CDS 1998 Jun 16 Antonio Claret Dos Santos <claret@iaa.es> J_A+A_335_647.xml Spectro-photometric evolution of elliptical galaxies. III. Infall models with gradients in mass density and star formation J/A+A/335/823 J/A+A/335/823 Evolution models of elliptical galaxies. III. Spectro-photometric evolution of elliptical galaxies. III. Infall models with gradients in mass density and star formation R Tantalo C Chiosi A Bressan P Marigo L Portinari Astron. Astrophys. 335 823 1998 1998A&A...335..823T J/A+A/311/361 : Evolution models of elliptical galaxies. II. (Tantalo+, 1996) Bressan et al., Paper I. 1994ApJS...94...63B Tantalo et al., Peper II. 1996, Cat. <J/A+A/311/361> Galaxies, photometry Models, evolutionary galaxies: abundances galaxies: elliptical and lenticular, cD galaxies: evolution galaxies: stellar content In this study we present a simple model of elliptical galaxies aimed at interpreting the gradients in colours and narrow band indices observed across these systems. Salient features of the model are the gradients in mass density and star formation and infall of primordial gas aimed at simulating the collapse of a galaxy into the potential well of dark matter. Adopting a multi-zone model we follow in detail the history of star formation, gas consumption, and chemical enrichment of the galaxy and also allow for the occurrence of galactic winds according to the classical supernova (and stellar winds) energy deposit. The outline of the model, the time scale of gas accretion and rate of star formation as a function of the galacto-centric distance in particular, seek to closely mimic the results from Tree-SPH dynamical models. Although some specific ingredients of the model can be questioned from many points of view (of which we are well aware), the model has to be considered as a gross tool for exploring the consequences of different recipes of gas accretion and star formation in which the simple one-zone scheme is abandoned. With the aid of this model we discuss the observational data on the gradients in metallicity, colours, and narrow band indices across elliptical galaxies.
Chemical Models at the Stage of Wind Ejection M(LT12) Asymptotic mass M_{L,T,12}_ solMass nu Efficiency of star formation {nu}(r_j/2_) --- zeta IMF parameter {zeta} --- tau Time scale of mass accretion {tau}(r_j/2_) Gyr M(Lt) Value reached by M_L,t_ at the onset of galactic wind solMass Age Age at which the galactic wind occurs, t_g{omega}_ Gyr G(rt) Dimensionless mass of gas G(r_j/2_,t) --- S(rt) Dimensionless mass of living stars S(r_j/2_,t) --- Zmax Maximum metallicity, Z(r_j/2_,t) Sun Zmean Mean metallicity, <Z(r_j/2_,t)> Sun Psi Rate of star formation {Psi}(r_j/2_,t) solMass/yr Omegag Gravitational binding energy of the gas {Omega}_g_(r_j/2_,t) --- Eg Total thermal energy of this E_g(r_j/2_,t) 10+43J ESNI Contributions to the thermal energy by Type I supernovae 10+43J ESNII Contributions to the thermal energy by Type II supernovae 10+43J ESW Contributions to the thermal energy by stellar winds; 10+43J r Mid shell fractionary radius r_j/2_ --- Integrated magnitude and colours of galaxy models M(lt12) Asymptotic mass of the model, M_l,t,12_ 10+12solMass nu Efficiency of star formation, {nu}(r_j/2_) --- tau Time scale of gas accretion, {tau}(r_j/2_) Gyr M(lt) Asymptotic mass of each zone, M_l,t_ 10+12solMass Age Age Gyr Mbol Integrated absolute bolometric of each zone mag Mvis Integrated visual magnitudes of each zone mag U-B Integrated colours (U-B) mag B-V Integrated colours (B-V) mag V-R Integrated colours (V-R) mag V-I Integrated colours (V-I) mag V-J Integrated colours (V-J) mag V-H Integrated colours (V-H) mag V-K Integrated colours (V-K) mag 1550-V Integrated colours (1550-V) mag Rad Fractionary radii r_j/2_ --- tables.tex LaTeX version of the tables tables.ps Post-Script version of the tables Patricia Bauer CDS 1998 May 26 Rosaria Tantalo <tantalo@pd.astro.it> J_A+A_335_823.xml Seyfert galaxies and environment: Seyferts in galaxy pairs and groups J/A+A/335/912 J/A+A/335/912 Seyferts in galaxy pairs and groups Seyfert galaxies and environment: Seyferts in galaxy pairs and groups B Kelm P Focardi G G C Palumbo Astron. Astrophys. 335 912 1998 1998A&A...335..912K VII/82 : Catalogue of isolated galaxies J/other/ApL/30.1 : Southern cat. of isolated pairs extension (Reduzzi+ 1995) Galaxies, Seyfert galaxies: interactions galaxies: Seyfert The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.
Seyferts in different samples Table Table number number=1 1: Seyferts in Karachentsev's (Cat. <VII/82>) isolated pairs 2: Seyferts in Reduzzi & Rampazzo's (1995ApL....30....1R) isolated pairs 3: Seyferts in Hickson's (1993ApL....29....1H) compact groups 4: Seyferts in Ramella, Huchra & Geller's (1989ApJ...344...57R) groups 5: Seyferts in Maia, Da Costa & Latham's (1989ApJS...69..809M) groups 6: Seyferts in Garcia's (1993Thesi.........G) groups --- Gal Galaxy Identificator --- Type Seyfert type number=2 Seyfert type is from Veron & Veron (1996, Cat. <VII/207>) catalog --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Pair/group Group and/or Pair Identificator and, within parenthesis, number of galaxies belonging to the group. number=3 Identification and number as from the original reference. --- pec Morphological peculiar appearance number=4 Morphological peculiarity has been derived via visual inspection of DSS and (in a few cases) of CCD R images taken at Loiano 152cm telescope. --- Ncomp Number of Seyfert close companions --- tables.ps Postscript version of the tables tables.tex LaTeX version of the tables Patricia Bauer CDS 1998 Jun 29 P. Focardi <PFOCARDI@astbo4.bo.astro.it> J_A+A_335_912.xml Spectral variability of the binary HR 4049 J/A+A/336/263 J/A+A/336/263 Radial velocities of HR 4049 Spectral variability of the binary HR 4049 E J Bakker D L Lambert H van Winckel J K McCarthy C Waelkens G Gonzalez Astron. Astrophys. 336 263 1998 1998A&A...336..263B J/A+A/306/924 : Optical spectrum of HR 4049 (Bakker+, 1996), Paper I. Line Profiles Radial velocities Stars, double and multiple binaries: close line: formation line: profiles stars: AGB and post-AGB stars: emission-line, Be stars: individual (HR 4049) The C I, Na I D, and H{alpha} lines of the post-AGB binary HR 4049 have been studied. Na I D variability results from a photospheric absorption component ([Na/H]=-1.6+/-0.2) which follows the velocity of the primary and a stationary, non-photospheric component. An emission component is attributed to the circumbinary disc, and an absorption component to mass-loss from the system with a velocity of 5.3+/-0.5km/s. The H{alpha} profile varies with the orbital period. The two strong shell type emission peaks are identified as from one single broad emission feature with an absorption centered around -7.5km/s. The intensity variations are largely attributed to a differential amount of reddening towards the H{alpha} emitting region and the stellar continuum. The radial velocities suggest that the H{alpha} emission moves in phase with the primary, but with a slightly lower velocity amplitude. From this we infer that the H{alpha} emission comes from outside the orbit of the primary, but still gravitationally bound to the primary. H{alpha} also shows a weak emission feature at -21.3+/-3.5km/s, which originates from the circumbinary disc and a weak absorption feature at -7.5+/-1.6km/s due to absorption by the circumbinary disc. We propose two competing models that could account for the observed velocity and intensity variations of the H{alpha} profile. Model I: light from the primary reflects on a localized spot near the inner radius of the circumbinary disc which is closest to the primary. Model II: H{alpha} emission originates in the outer layers of the extended atmosphere of the primary due to activity. These activities are locked to the position of the primary in its orbit. We discuss the similarities of variability and shape of the H{alpha} emission of HR 4049 with those of early type T-Tauri stars (e.g SU Aur).
HR 4049 HD 89353 10 18 07.6 -28 59 32
Log of 32 Na I D observations Log of 60 H{alpha} observations Date Observation date "DD/MM/YY" HJD Heliocentric Julian date d {phi}abs Phase number=1 {phi}abs=0.0 at HJD=T_0_=2446746.6+/-2.4 --- Tel/Instr Telescope/Instrument number=2 CAT/CES: Twenty-three H{alpha} and two Na I D single-order spectra (R~55,000) have been obtained by HvW and CW on the ESO observatory at La Silla (Chili) using the coude echelle spectrograph at the 1.4m Coude Auxiliary Telescope. McD/CS11: Twenty-three H{alpha} and twenty-one Na I D single-order spectra (R~60,000) have been obtained by DLL, JKM, and Jos Tomkin using the echelle spectrograph (6-foot camera) on the 2.7m McDonald telescope. McD/CE: Ten multi-order spectra (R~45,000) have been obtained by GG using the Sandiford cassegrain echelle spectrograph (McCarthy et al., 1993PASP..105..881M) on the 2.1m McDonald telescope. Eight contain H{alpha} and four Na I D. WHT/UES: Three multi-order spectra (R~50,000) have been obtained in service time using the Utrecht echelle spectrograph on the 4.2m William Herschel telescope on La Palma (Unger, 1994, La Palma Technical Notes No. XXIII). All three spectra contain H{alpha}, Na I D, and numerous photospheric absorption lines. An extensive analysis of these spectra and complete line identification have been published in Paper I (Bakker et al., 1996, Cat. <J/A+A/306/924>). McD/CS21: Two multi-order spectra (R~160,000) have been obtained by EJB using the cross-dispersed echelle spectrograph (Tull et al., 1995PASP..107..251T) at the 2.7m McDonald telescope. Both contain H{alpha} and Na I D. CTIO/ES: One single-order H{alpha} spectrum (R~18,000) has been obtained by Andy McWilliam using the echelle spectrograph with the air Schmidt camera on the 4m CTIO telescope. --- R Spectral resolving power --- HRV Heliocentric radial velocity number=3 In table3.dat, heliocentric radial velocities are computed using the orbital parameters In table4.dat, heliocentric radial velocities are measured from CI, N I, and O I lines; the velocity accuracy is 2km/s km/s tables.tex LaTeX version of the tables fig12.ps *Observed NaI D_2_ line profiles in order of relative orbital phase {phi}_rel_ The systemic velocity of the binary, {gamma}_s_=-32.15km/s, is at zero (solid line) with on both sides a short-dashed line at the extreme velocity of the star in its orbit. The long-dashed lines correspond to the velocity of that star. The measured velocities and intensities of the marker points are marked. The photospheric component (on the profile, only if measured) and the predicted stellar velocity (at an intensity of 1.0) have both been plotted with a dot. These two points can be at different velocities because the photospheric velocity cannot be very well determined from the observed NaI D_2_ profile. The circumsystem markers (diamond and triangle) and the interstellar markers (crosses) have been marked. In each window, the upper left corner gives the absolute orbital phase and the upper right corner the telescope/instrument with which the spectrum was obtained. fig13.ps Figure 12 continued fig14.ps *Observed H{alpha} line profiles in order of relative orbital phase {phi}_rel_ The systemic velocity of the binary, {gamma}_s_=-32.15km/s, is at zero (solid line) with on both sides a short-dashed line at the extreme velocity of the star in its orbit. The long-dashed lines correspond to the velocity of that star. The "blue maximum" (cross), "blue minimum" (open square), "central maximum" (open triangle), "red minimum" (open diamond), and "red maximum" (asterisk) have been marked. In each window, the upper left corner gives the absolute orbital phase and the upper right corner the telescope/instrument with which the spectrum was obtained. fig15.ps Figure 14 continued fig16.ps Figure 14 continued fig17.ps Figure 14 continued Patricia Bauer CDS 1998 Mar 05 Eric J. Bakker <ebakker@astro.as.utexas.edu> J_A+A_336_263.xml A search for precursors of ultracompact HII regions in a sample of luminous IRAS sources. II. VLA observations. J/A+A/336/339 J/A+A/336/339 VLA observations of ultracompact HII regions A search for precursors of ultracompact HII regions in a sample of luminous IRAS sources. II. VLA observations. S Molinari J Brand R Cesaroni F Palla G G C Palumbo Astron. Astrophys. 336 339 1998 1998A&A...336..339M J/A+A/308/573 : Ammonia on YSOs IRAS sources, Paper I. (Molinari+ 1996) Infrared sources Radio sources YSOs circumstellar matter HII regions radio continuum: ISM stars: formation stars: pre-main sequence We have used the Very Large Array (VLA) to search for radio continuum emission towards a sample of 67 IRAS sources selected from a previous study. All observed sources are associated with high density molecular gas, exhibit an infrared spectral energy distribution characteristic of very cold young stellar objects and many of them are associated with H_2_O masers. The observed sample is divided into two groups of sources: High, with IRAS spectral energy distributions resembling those of ultracompact HII regions, and Low, for which previously collected evidence suggests that they may contain a higher fraction of protostellar objects than the High group; such objects might not have started hydrogen burning yet. Radio continuum emission was detected towards 37 sources (55%), although only in 22 cases an association with the IRAS source is established. Of the latter, 9 (24%) objects belong to the Low type and 13 (43%) to the High type. Thus, we find that 76% of Low and 57% of High sources are not associated with a radio counterpart. Because the majority of the sources have luminosities above ~10^4^L_{sun}_, corresponding to central stars of spectral type between B2 and O7, the lack of radio emission is interpreted as being due to the action of accreting matter that chokes off the expansion of the ionised gas. We show that this require s only moderate mass accretion rates, below ~10^-4^M_{sun}_/yr. Alternatively, dust absorption can also effectively absorb UV photons and the gas column density implied by our observations indicates values in excess of 10^22^cm^-2^. The physical properties of IRAS sources with associated radio counterpa rt derived from the present observations do not distinguish between High and Low sources. These sources are likely to be ZAMS stars with variable amounts of dust within the ionised region which acts as UV field absorber. The large majority of detected sources (75%) have spherical or unresolved morphology, while 15% are irregular or multiply peaked and only 10% have a core-halo structure. These results agree with the known properties of ultracompact HII regions, even though the average luminosity of the present sample is an order of magnitude lower than that in previous studies.
High sources at 6-cm (obs. data) Low sources at 2 and 6-cm (obs. data) Mol Molinari number from Paper I (Cat. <J/A+A/308/573>) --- Ass An * indicates association of radio emission with the IRAS source --- Com Identification of multiple components within a source, or multiple sources within a field --- Lam Wavelength of observation cm Run Code for observing run number=1 I: 26 June 1994 II: 4 Oct. 1994 III: 23-24 Jan. 1995 --- RAh Right ascension (1950) number=2 When there is no positions, the source has not been detected h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Sign of declination --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Sep Angular distance radio- and IRAS sources arcsec Note1 Note number=3 A "(" in this column, and a ")" in column 110 indicate that the values of all parameters in between refer to the image that has been degraded to the resolution of the other (lower resolution) image. --- Maj Observed major axis of radio peak arcsec Min Observed minor axis of radio peak arcsec PA Position angle radio peak (E of N) deg Majd Major axis radio peak, deconvolved by beam arcsec Mind Minor axis radio peak, deconvolved by beam arcsec PAd Position angle deconvolved radio peak (E of N) deg Ha1 Size of halo in one direction number=4 Halo: extended component above 2 {sigma} level arcsec --- --- Ha2 Size of halo in other direction arcsec Mc Morphological class number=5 S = spherical/unresolved CH = Core-Halo I = irregular/multiply peaked --- l_F To indicate next number is upper limit --- F Observed peak flux density (mJy/beam) mJy S Observed integrated flux mJy rms Observed rms (mJy/beam) number=6 If no value is listed, the theoretical rms (0.15 mJy/beam) is assumed mJy --- See note number=3 A "(" in this column, and a ")" in column 110 indicate that the values of all parameters in between refer to the image that has been degraded to the resolution of the other (lower resolution) image. --- Note Individual notes in note1a.dat or note1b.dat --- High sources at 6-cm derived physical parameters Low sources at 2 and 6-cm derived phys. parameters Mol Molinari number from Paper I (Cat. <J/A+A/308/573>) --- Ass An * indicates association of radio emission with the IRAS source --- Com Identification of multiple components within a source, or multiple sources within a field --- Lam Wavelength of observation cm Note1 Note number=1 A "(" in this column, and a ")" in column 68 indicate that the values of all parameters in between refer to the image that has been degraded to the resolution of the other (lower resolution) image. --- l_DiamP To indicate DiamP is upper limit --- DiamP Peak diameter pc DiamH Mean halo diameter pc Tb Brightness temperature K tau Optical depth * 1000. --- l_Ne To indicate ne is lower limit --- Ne Electron density 10+4cm-3 l_EM To indicate EM is lower limit --- EM Emission measure 10+6pc/cm6 l_M(Hii) To indicate M(Hii) is upper limit --- M(Hii) Mass of ionized hydrogen 10-3solMass log(Nly) Log10 of Lyman continuum flux [s-1] --- See note number=1 A "(" in this column, and a ")" in column 68 indicate that the values of all parameters in between refer to the image that has been degraded to the resolution of the other (lower resolution) image. --- Rat Ratio of integrated and peak fluxes --- SpI Spectral index --- Note Comments --- Individual notes to table1a.dat Individual notes to table1b.dat Mol Mol number --- Com Identification of multiple components --- Ntot Total number of lines for the comment --- Nline Running line number in range [1,Ntot] --- Comm Comment --- map/* titles Mol Mol number --- FileName map name, stored in subdirectory map --- Title Title of the map --- Patricia Bauer CDS 1998 May 22 Sergio Molinari <molinari@ipac.caltech.edu> Jan Brand <BRAND@astbo1.bo.cnr.it> J_A+A_336_339.xml The supercluster-void network. IV. The shape and orientation of superclusters. J/A+A/336/35 J/A+A/336/35 Shape and orientation of superclusters The supercluster-void network. IV. The shape and orientation of superclusters. J Jaaniste E Tago M Einasto J Einasto H Andernach V Mueller Astron. Astrophys. 336 35 1998 1998A&A...336...35J J/A+AS/123/119 : The supercluster-void network. I. (Einasto+ 1997) Einasto, M., Tago, E., Jaaniste, J., Einasto, J., Andernach, H., 1997A&AS..123..119E (Paper I) Einasto, M., Frisch, P., Gottloeber, S., Mueller, V., Saar, V., Starobinsky, A.A., Tago, E., Tucker, D., Andernach, H., 1997MNRAS.289..801E (Paper II) Einasto, M., Frisch, P., Gottloeber, S., Mueller, V., Saar, V., Starobinsky, A.A., Tucker, D., 1997MNRAS.289..813E (Paper III) Clusters, galaxy cosmology: observations galaxies: clusters: general large-scale structure of universe We present a study of the shape, size, and spatial orientation of superclusters of galaxies. Approximating superclusters by triaxial ellipsoids we show that superclusters are flattened, triaxial objects. We find that there are no spherical superclusters. The sizes of superclusters grow with their richness: the median semi-major axis of rich and poor superclusters (having >=8 and <8 member clusters) is 42 and 31h^-1^Mpc, respectively. Similarly, the median semi-minor axis is 12 and 5h^-1^Mpc for rich and poor superclusters. The spatial orientation of superclusters, as determined from the axes of the ellipsoids, is nearly random. We do not detect any preferable orientation of superclusters, neither with respect to the line of sight, nor relative to some other outstanding feature in the large scale structure, nor with respect to the directions of principal axes of adjacent superclusters.
Shape and orientation of superclusters SCL Supercluster number, as in Cat. J/A+AS/123/119 --- nCl Number of clusters in supercluster --- a First semiaxis of concentration ellipsoid Mpc b Second semiaxis of concentration ellipsoid Mpc c Third semiaxis of concentration ellipsoid Mpc V/Vsph Ratio of ellipsoid to sphere volumes (bc/a^2^) --- Xa Angle of a-axis with the supergalactic X-axis deg Xc Angle of c-axis with the supergalactic X-axis deg Ra Angle of a-axis with the line of sight deg Rc Angle of c-axis with the line of sight deg RAdeg Right ascension (1950) of supercluster centre position taken from Cat. J/A+AS/123/119 deg DEdeg Declination (1950) of supercluster centre deg Heinz Andernach Univ. Guanajuato Francois Ochsenbein CDS 1999 Jul 21 UNKNOWN UNKNOWN * 21-Jul-1999: received from Heinz Andernach (heinz@astro.ugto.mx) who prepared the table from the latex manuscript (astro-ph/9807044). Equatorial coordinates were added to this table at CDS. J_A+A_336_35.xml The planetary nebulae populations in five galaxies: abundance patterns and evolution J/A+A/336/667 J/A+A/336/667 PN abundances in five galaxies The planetary nebulae populations in five galaxies: abundance patterns and evolution G Stasinska M G Richer M L McCall Astron. Astrophys. 336 667 1998 1998A&A...336..667S Abundances Opacities Planetary nebulae galaxies: abundances planetary nebulae: general stars: AGB and post-AGB We have collected photometric and spectroscopic data on planetary nebulae (PNe) in 5 galaxies: the Milky Way (bulge), M31 (bulge), M 32, the LMC and the SMC. We have computed the abundances of O, Ne and N and compared them from one galaxy to another. In each Galaxy, the distribution of oxygen abundances has a large dispersion. The average O/H ratio is larger in the M31 and the Galactic bulge PNe than in those in the Magellanic Clouds. In a given galaxy, it is also larger for PNe with [OIII] luminosities greater than 100L_{sun}_, which are likely to probe more recent epochs in the galaxy history. We find that the M31 and the Galactic bulge PNe extend the very tight Ne/H-O/H correlation observed in the Galactic disk and Magellanic Clouds PNe towards higher metallicities. We note that the anticorrelation between N/O and O/H that was known to occur in the Magellanic Clouds and in the disk PNe is also marginally found in the PNe of the Galactic bulge. Furthermore, we find that high N/O ratios are higher for less luminous PNe. In M 32, all PNe have a large N/O ratio, indicating that the stellar nitrogen abundance is enhanced in this galaxy. We have also compared the PN evolution in the different galactic systems by constructing diagrams that are independent of abundances, and have found strikingly different behaviours of the various samples. In order to help in the interpretation of these data, we have constructed a grid of expanding, PN photoionization models in which the central stars evolve according to the evolutionary tracks of Bloecker (1995A&A...299..755B). These models show that the apparent spectroscopic properties of PNe are extremely dependent, not only on the central stars, but also on the masses and expansion velocities of the nebular envelopes. The main conclusion of the confrontation of the observed samples with the model grids is that the PN populations are indeed not the same in the various parent galaxies. Both stars and nebulae are different. In particular, the central stars of the Magellanic Clouds PNe are shown to evolve differently from the hydrogen burning stellar evolutionary models of Bloecker (1995). In the Galactic bulge, on the other hand, the behaviour of the observed PNe is roughly compatible with the theoretical stellar evolutionary tracks. The case of M31 is not quite clear, and additional observations are necessary. It seems that the central star mass distribution is narrower for the M31 PNe than for the Galactic bulge PNe. We show that spectroscopy of complete samples of PNe down to a factor 100 below the maximum luminosity would help to better characterize the PN central star mass distribution.
Reddening corrected line intensities on the scale I(H{beta})=100 and logarithms of [OIII] luminosities in solar units Region Region number=1 Region takes the values a: M 31 b: Milky Way bulge c: M 32 d: LMC e: SMC --- Object Object number --- PN PN name ---- Ref Reference number=2 M31, M32: a Richer, Stasinska, McCall, 1998, A&AS, submitted Milky Way bulge: a Aller & Keyes, 1987ApJS...65..405A b Webster, 1988MNRAS.230..377W c Ratag et al., 1997, Cat. <J/A+AS/126/297> LMC: a Meatheringham & Dopita, 1991, Cat. <J/ApJS/75/407> b Meatheringham & Dopita, 1991, Cat. <J/ApJS/76/1085> c Jacoby & Kaler, 1993ApJ...417..209J d Boroson & Liebert, 1989ApJ...339..844B e Leisy & Dennefeld, 1996, Cat. <J/A+AS/116/95> f Monk, Barlow & Clegg, 1988, Cat. <J/MNRAS/234/583> g Vassiliadis et al., 1992, Cat. <J/ApJS/83/87> m Jacoby, Walker & Ciardullo, 1990ApJ...365..471J o Wood et al., 1987ApJ...320..178W s Meatheringham, Dopita & Morgan, 1988ApJ...329..166M SMC: a Aller et al., 1981MNRAS.194..613A b Barlow, 1987MNRAS.227..161B c Boroson & Liebert, 1989ApJ...339..844B d Jacoby & Kaler, 1993ApJ...417..209J e Leisy & Dennefeld, 1996, Cat. <J/A+AS/116/95> f Meatheringham & Dopita, 1991, Cat. <J/ApJS/75/407> g Meatheringham & Dopita, 1991, Cat. <J/ApJS/76/1085 h Meyssonnier, 1995A&AS..110..545M i Monk, Barlow & Clegg ,1988, Cat. <J/MNRAS/234/583> j Vassiliadis et al., 1992, <J/ApJS/83/87> k Meatheringham et al., 1990ApJ...361..101M --- l_3727 Limit flag on 3727 --- 3727 Reddening corrected line intensity at 3727AA number=3 H{beta}=100 --- u_3727 Uncertainty flag on 3727 --- 3869 Reddening corrected line intensity at 3869AA number=3 H{beta}=100 --- u_3869 Uncertainty flag on 3869 --- l_4363 Limit flag on 4363 --- 4363 Reddening corrected line intensity at 4363AA number=3 H{beta}=100 --- u_4363 Uncertainty flag on 4363 --- l_4686 Limit flag on 4686 --- 4686 Reddening corrected line intensity at 4686AA number=3 H{beta}=100 --- u_4686 Uncertainty flag on 4686 --- l_5007 Limit flag on 5007 --- 5007 Reddening corrected line intensity at 5007AA number=3 H{beta}=100 --- u_5007 Uncertainty flag on 5007 --- l_5755 Limit flag on 5755 --- 5755 Reddening corrected line intensity at 5755AA number=3 H{beta}=100 --- u_5755 Uncertainty flag on 5755 --- l_5876 Limit flag on 5876 --- 5876 Reddening corrected line intensity at 5876AA number=3 H{beta}=100 --- u_5876 Uncertainty flag on 5876 --- l_6300 Limit flag on 6300 --- 6300 Reddening corrected line intensity at 6300AA number=3 H{beta}=100 --- u_6300 Uncertainty flag on 6300 --- 6563 Reddening corrected line intensity at 6563AA number=3 H{beta}=100 --- l_6583 Limit flag on 6583 --- 6583 Reddening corrected line intensity at 6583AA number=3 H{beta}=100 --- u_6583 Uncertainty flag on 6583 --- l_6717 Limit flag on 6717 --- 6717 Reddening corrected line intensity at 6717AA number=3 H{beta}=100 --- u_6717 Uncertainty flag on 6717 --- l_6731 Limit flag on 6731 --- 6731 Reddening corrected line intensity at 6731AA number=3 H{beta}=100 --- u_6731 Uncertainty flag on 6731 --- 7325 Reddening corrected line intensity at 7325AA number=3 H{beta}=100 --- u_7325 Uncertainty flag on 7325 --- logL5007 [OIII] luminosity [Sun] Electron temperatures and densities, elemental and ionic abundances Region Region --- Object Object number --- PN NP name --- He/H He/H abundance ratio --- N/H N/H abundance ratio --- O/H O/H abundance ratio --- Ne/H Ne/H abundance ratio --- ne(SII) Electronic density deduced from [S II]6717/6730 cm-3 T(O3) Electronic temperature deduced from [O III]4363/5007 K T(N2) Electronic temperature deduced from [N II]5755/6584 K O+3727/H O^+^/H value deduced from [O II]3727/H{beta} --- O+7325/H O^+^/H value deduced from [O II]7325/H{beta} --- O++/H O^++/H abundance ratio --- N+/H N^+/H abundance ratio --- Ne++/H Ne^++^/H abundance ratio --- He+/H He^+^/H abundance ratio --- He++/H He^++^/H abundance ratio --- Patricia Bauer CDS 1998 May 28 Grazyna Stasinska <grazyna@obspm.fr> J_A+A_336_667.xml HD 163151: a new W UMa type system J/A+A/336/920 J/A+A/336/920 HD 163151: a new W UMa type system HD 163151: a new W UMa type system E Rodriguez A Claret J M Garcia F M Zerbi R Garrido S Martin C Akan K Luedeke V Keskin C Ibanoglu S Evren Z Tunca R Pekunlu M Paparo J Nuspl K Krisciunas S Y Jiang Astron. Astrophys. 336 920 1998 1998A&A...336..920R Binaries, eclipsing Photometry, UBV Photometry, uvby, beta binaries: visual stars: fundamental parameters stars: individual (HD 163151) techniques: photometric Table 2 contains 408 simultaneous measurements collected in each of the four uvby colours of the Stromgren photometric system for the W UMa system HD 163151. The data are magnitude differences (Du, Dv, Db, Dy, D(b-y), Dm1, Dc1) of the variable star minus comparison star in the standard system versus Heliocentric Julian Day. Tables 3, 4 and 5 are the same, but for H{beta} (65 points), Johnson B data (212 points) and Johnson V data (355 points). The comparison star is HD 166095. The origin in time is the Julian Day 2449858. The observations were carried out (by E. Rodriguez, A. Claret, J.M. Garcia, F.M. Zerbi, R. Garrido, S. Martin, C. Akan, K. Luedeke, V. Keskin, C. Ibanoglu, S. Evren, Z. Tunca, R. Pekunlu, M. Paparo, J. Nuspl, K. Krisciunas and S.Y. Jiang) in 1995 during the course of a multisite campaign. The following telescopes were used: 90cm telescope of the Sierra Nevada Observatory, Spain (uvby-H{beta} photometry); 50cm telescope at the Ege University Observatory, Turkey (BV-uvby); 50cm telescope at Piszkesteto mountain station, Konkoly Observatory, Hungary (BV); 50cm telescope at the Merate Observatory, Italy (V); 30cm telescope at Albuquerque, New Mexico, USA (V) and 15cm telescope at Mauna Kea, Hawaii, USA (V).
HD 163151 17 54 14.2 +11 07 58 HD 166095 18 08 33.6 +14 17 04
ubvy differential photometry HJD Heliocentric Julian date d Dumag u magnitude difference (var. minus comp.) mag Dvmag v magnitude difference (var. minus comp.) mag Dbmag b magnitude difference (var. minus comp.) mag Dymag y magnitude difference (var. minus comp.) mag Db-y b-y colour index difference (var. minus comp.) mag Dm1 m1 colour index difference (var. minus comp.) mag Dc1 c1 colour index difference (var. minus comp.) mag H{beta} differential photometry HJD Heliocentric Julian date d Hbeta H{beta} index difference (var. minus comp.) mag B differential photometry HJD Heliocentric Julian date d Bmag B magnitude difference (var. minus comp.) mag V differential photometry HJD Heliocentric Julian date d Vmag V magnitude difference (var. minus comp.) mag Patricia Bauer CDS 1998 Jun 02 Eloy rodriguez <eloy@iaa.es> J_A+A_336_920.xml The HR diagram form Hipparcos data. Absolute magnitudes and kinematics of Bp-Ap stars. J/A+A/336/953 J/A+A/336/953 Bp-Ap stars HR-diagram from Hipparcos data The HR diagram form Hipparcos data. Absolute magnitudes and kinematics of Bp-Ap stars. A E Gomez X Luri S Grenier F Figueras P North F Royer J Torra M -O Mennessier Astron. Astrophys. 336 953 1998 1998A&A...336..953G I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) magnitudes, absolute Stars, Ap Stars, Bp Stars, distances Hertzsprung-Russell (HR diagram) stars: chemically peculiar stars: distances stars: fundamental parameters stars: kinematics Using Hipparcos (Cat. <I/239>) parallaxes and proper motions together with radial velocity data, the luminosity calibration and kinematics of Bp-Ap stars have been obtained. The used statistical method allows to treat inhomogeneous samples and to identify the different groups. Six types of Bp-Ap stars (He-rich, He-weak, Hg-Mn, Si, Si+ and SrCrEu) have been considered. In most of the samples, with the exception of the He-rich and He-weak stars, two groups have been separated. Individual distances and luminosities are given for the stars belonging to the main groups which contain the largest number of stars. The list of stars in the secondary groups is given
Individual estimations for main group stars HIP HIPPARCOS (Cat. <I/239>) number --- HD HD (Cat. <III/135>) number --- Prob Probability of belonging to the group % Dist Distance pc e_Dist Distance error pc Vmag Apparent V-magnitude mag MVmag Absolute visual magnitude mag Class Spectral Classification --- List of stars in the secondary groups HIP HIPPARCOS (Cat. <I/239>) number --- HD HD (Cat. <III/135>) number --- Prob Probability of belonging to the group % Class Spectral Classification --- Patricia Bauer CDS 1998 Aug 03 Anita Gomez <anita@mehipp.obspm.fr> J_A+A_336_953.xml HD 37017 = V1046 Ori. A double-lined spectroscopic binary with a B2e He-strong magnetic primary J/A+A/337/183 J/A+A/337/183 V1046 Ori uvby photometry and radial velocities HD 37017 = V1046 Ori. A double-lined spectroscopic binary with a B2e He-strong magnetic primary C T Bolton P Harmanec R W Lyons A P Odell D M Pyper Astron. Astrophys. 337 183 1998 1998A&A...337..183B Binaries, spectroscopic Photometry, uvby Radial velocities binaries: spectroscopic stars: fundamental parameters stars: individual (HD 37017, V1046 Ori) stars: oscillations We report on a detailed spectroscopic and photometric study of V1046 Orionis undertaken to resolve uncertainties about the period(s) and causes of the spectroscopic and photometric variations of this helium-strong star. We have detected the lines of the secondary star in an extensive series of photographic and electronic spectra. This eliminates any doubt about the duplicity of this star. The orbital elements we derive from our measures of these spectra confirm the unusually large orbital eccentricity, e=0.433, for the short, P=18.65612d, orbital period. The line profiles, V/R ratio of the double H{alpha} emission, residuals of the primary radial velocities from the orbital velocity curve, brightness and colour of the object, magnetic field, and radio emission of this system all vary with a period of 0.9011836d. We tentatively follow earlier investigators in interpreting this as the rotational period of the primary and summarize the evidence of the phase shifts among the different phenomena, using the accurate value of the 0.9d period, to put tight constraints on any future model of these changes. We postpone our own attempt at a quantitative modelling of the variations with the 0.9d period for a separate study.
V1046 Ori HD 37017 HR 1890 05 35 21.8 -04 29 38
V1046 Ori individual uvby photometric observations from several stations HJD Heliocentric Julina date d ymag y magnitude mag bmag b magnitude mag umag u magnitude mag vmag v magnitude mag b-v b-v colour index mag u-b u-b colour index mag c1 c1 colour index mag m1 m1 colour index mag Obs Observing station code number=1 Numbers in column `Obs" correspond to those in column "Instrument" of Table 2: 1: Catalina station of Lunar and Planetary Lab. Johnson et al. 1966, Cat. <II/5> 2: 0.5-m reflector, Sutherland, South Africa (Balona, priv. com.) 4: Danish 0.5-m reflector, La Silla (Maitzen, 1981, priv.com.) 6: 0.8-m Four College Automatic photoelectric telescope, USA --- V1046 Ori radial velocities measured on David Dunlap photographic spectra HJD Heliocentric Julian date d RV1(H+He) Measured radial velocity for mean H+He km/s RV1(HeI) Measured radial velocity for HeI km/s RV1(He416.9) Measured radial velocity for He 416.9 km/s RV2(MgII) Measured radial velocity for Mg II km/s RV(CaII) Measured radial velocity for Ca II km/s FWHM Full widths at half maximum of He 447.1 nm Ic Central intensity of He 447.1 --- EW Equivalent width of He 447.1 nm tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Jun 12 Petr Harmanec <hec@sunstel.asu.cas.cz> C. Tom Bolton <bolton@struve.astro.utoronto.ca> J_A+A_337_183.xml Evolutionary models for solar metallicity low-mass stars: mass-magnitude relationships and color-magnitude diagrams J/A+A/337/403 J/A+A/337/403 Low-mass stars evolutionary models Evolutionary models for solar metallicity low-mass stars: mass-magnitude relationships and color-magnitude diagrams I Baraffe G Chabrier F Allard P Hauschildt Astron. Astrophys. 337 403 1998 1998A&A...337..403B J/A+A/327/1039 : Structure and evolution of low-mass stars (Chabrier+ 1997) Models, evolutionary Photometry Stars, masses Hertzsprung-Russell (HR diagram) stars: atmospheres stars: evolution stars: interiors stars: low-mass, brown dwarfs Physical properties and absolute magnitudes of low-mass stars for different initial metallicity [M/H], helium mass fraction Y and mixing length parameter Lmix: mass (in solar mass), age (in Gyrs) effective temperature (in K), log of gravity (in cgs) and absolute magnitudes. The VRI magnitudes are in the Johnson-Cousins system and the JHK magnitudes in the CIT system. Note that the bolometric magnitude corresponds to M_bol(Sun)=4.64. The lowest mass corresponds to the hydrogen-burning limit.
Evolutionary models [M/H] Initial metallicity (0 or -0.5) [Sun] Y Initial helium mass fraction (0.275, 0.25 or 0.282) Sun Lmix Initial mixing length parameter (in H_P_) --- Mass Mass number=1 The lowest mass corresponds to the hydrogen-burning limit solMass Age Age Gyr Teff Effective temperature K logg Gravity [cm/s2] Mbol Absolute bolometric magnitude number=2 The bolometric magnitude corresponds to M_bol (Sun) = 4.64 mag MV Absolute V (Johnson-Cousins system) magnitude mag MR Absolute R (Johnson-Cousins system) magnitude mag MI Absolute I (Johnson-Cousins system) magnitude mag MJ Absolute J (CIT system) magnitude mag MH Absolute H (CIT system) magnitude mag MK Absolute K (CIT system) magnitude mag Patricia Bauer CDS 1998 Jul 30 Isabelle Baraffe <Isabelle.Baraffe@ens-lyon.fr> J_A+A_337_403.xml The pulsating yellow supergiant V810 Centauri J/A+A/337/779 J/A+A/337/779 V810 Cen Geneva photometry The pulsating yellow supergiant V810 Centauri F Kienzle G Burki M Burnet G Meynet Astron. Astrophys. 337 779 1998 1998A&A...337..779K II/169 : Catalogue of observations in the Geneva photometric system Photometry, Geneva Stars, supergiant open clusters and associations: individual (Stock 14) stars: evolution stars: individual (V810 Cen) stars: oscillations supergiants The light curve of the yellow supergiant V810 Centauri in the Geneva photometric system has been analysed with Date Compensate Fourier Transform and Weighted Wavelet Z-transform. Two periods around 150 and 100 days dominate the frequency spectrum but variable amplitudes and other modes are required to fully reproduce whole data set.
V810 Cen HD 101947 11 43 31.2 -62 29 21
The photometric measurements of V810 Cen in the Geneva system HJD Heliocentric Julian day d q Photometric Q weight (Rufener 1988, Cat. <II/169>) --- Vmag Magnitude in the visible mag p Photometric P weight (Rufener 1988, Cat. <II/169>) --- [U-B] Geneva [U-B] index mag [V-B] Geneva [V-B] index mag [B1-B] Geneva [B1-B] index mag [B2-B] Geneva [B2-B] index mag [V1-B] Geneva [V1-B] index mag [G-B] Geneva [G-B] index mag Fz Airmass --- Patricia Bauer CDS 1998 Jun 23 Francesco Kienzle <Francesco.Kienzle@obs.unige.ch> J_A+A_337_779.xml Spectral evolution of Nova (V723) Cassiopeiae 1995: pre-maximum stage. J/A+A/338/1006 J/A+A/338/1006 V723 Cas equivalent widths Spectral evolution of Nova (V723) Cassiopeiae 1995: pre-maximum stage. T Iijima L Rosino M Della Valle Astron. Astrophys. 338 1006 1998 1998A&A...338.1006I Equivalent widths Novae novae, cataclysmic variables stars: individual (V723 Cas) stars: late-type stars: low-mass, brown dwarfs The monitoring of spectral evolution of the very slow nova V723 Cas started at the Asiago Astrophysical Observatory just on the announcement of discovery. In this paper the spectral evolution during the long pre-maximum stage, which lasted from August to December 1995, is reported. Emission lines of H I and Fe II were prominent in the early stage. Most of the lines were accompanied by P Cygni type absorption components. The emission lines gradually weakened with time and the absorption components developed. The mean of the blue-shifts of the absorption components with respect to the emissions was about -126km/s in September and -96km/s in December 1995. Some lines of Fe I, Fe II, Y II, Sc II, Ba II, etc. appeared in the later stage. All emission lines, except for H{alpha}, once nearly disappeared in November when the nova slightly brightened to V=~8.6. Some emission lines appeared again several days before the beginning of the final rise to maximum luminosity, then a pure absorption spectrum of F type supergiant was seen on the maximum of V=~7.1 at the middle of December. The absorption components of Si II lines at 634.7 and 637.1nm showed fairly different profiles from those of the other metallic lines, which suggests a complicated gas motion in the atmosphere. The distance and the absolute magnitude at maximum are estimated to be 2.95+/-0.7kpc and M_V_(max)=-6.1+/-0.5, respectively. The mass of the white dwarf in this system may be about 0.58+/-0.07M_{sun}_.
V723 Cas NOVA Cas 1995 01 05 05.4 +54 00 40
Wavelengths, equivalent widths and identifications of all emission and absorption lines of Nova (V723) Cas 1995 observed on 1995 Sept. 12 and Dec. 4 lambda1 Measured wavelength on 12/09/95 0.1nm EW1 Equivalent width (12/09/95) 0.1nm u_EW1 Uncertainty flag on EW1 --- lambda2 Measured wavelength on 04/12/95 0.1nm EW2 Equivalent width (04/12/95) 0.1nm u_EW2 Uncertainty flag on EW2 --- Ident Identification number=1 Identifications of the lines, where the name of ions, multiplet numbers, and their laboratory wavelengths are presented, but the first two digits of the wavelengths are omitted. --- Patricia Bauer CDS 1998 Jul 31 Takashi Iijima <iijima@astras.pd.astro.it> J_A+A_338_1006.xml Optical spectroscopy of DENIS Mini-Survey Brown Dwarf Candidates. J/A+A/338/1066 J/A+A/338/1066 Optical Spectra of DENIS Brown Dwarf Candidate Optical spectroscopy of DENIS Mini-Survey Brown Dwarf Candidates. C G Tinney X Delfosse T Forveille F Allard Astron. Astrophys. 338 1066-1072 1998 1998A&A...338.1066T Spectroscopy Stars, dwarfs Stars, late-type stars: late-type stars: low-mass, brown dwarfs Optical spectra for candidate brown dwarfs from the DENIS Mini-survey are provided. These are the spectra used to in Figure 1 of the paper.
These data were acquired with the Anglo-Australian Telescope and the RGO Spectrograph. The FWHM resolution is 0.7nm at a dispersion of 0.34nm. Wavelength coverage extends from 648nm to 989nm. Atmospheric absorption is not corrected, making the data longward of 920nm suspect. BRI 0021-0214, file "bri0021.dat" 00 24 24.5 -01 58 21 GRH 2208, file "grh2208.dat" 22 10 50.0 -19 52 13 DENIS-P J0020-4414, file "j0020-44.dat" 00 20 59.4 -44 14 43 DENIS-P J0021-4244, file "j0021-42.dat" 00 21 05.7 -42 44 50 DENIS-P J0205-1159, file "j0205-11.dat" 02 05 29.0 -11 59 25 DENIS-P J1058-1548, file "j1058-15.dat" 10 58 46.6 -15 48 00 DENIS-P J1228-1547, file "j1228-15.dat" 12 28 13.8 -15 47 11 DENIS-P J2040-3245, file "j2040-32.dat" 20 40 06.2 -32 45 24 DENIS-P J2052-5512, file "j2052-55.dat" 20 52 55.0 -55 12 03 DENIS-P J2146-2153, file "j2146-21.dat" 21 46 10.6 -21 53 09 VB 10 GJ 752B LHS 474, file "vb10.dat" 19 16 59.9 +05 10 18
Spectrum for BRI0021-0214 Spectrum for GRH2208 Spectrum for DENIS-P J0020-4414 Spectrum for DENIS-P J0021-4244 Spectrum for DENIS-P J0205-1159 Spectrum for DENIS-P J1058-1548 Spectrum for DENIS-P J1228-1547 Spectrum for DENIS-P J2040-3245 Spectrum for DENIS-P J2052-5512 Spectrum for DENIS-P J2146-2153 Spectrum for VB10 Lambda Central wavelength of the flux bin 0.1nm Fnu Flux number=1 Data in interorder gaps has value 0.0 Units are erg/cm**2/s/A, but have been normalised to have value mean value 1.0 in the wavelength range 830-840nm mJy N. Paul Kuin SSDOO/ADC Patricia Bauer CDS 1999 Mar 09 Gail L. Schneider <gschneid@pop600.gsfc.nasa.gov> J_A+A_338_1066.xml Asteroids as far-infrared photometric standards for ISOPHOT J/A+A/338/340 J/A+A/338/340 Asteroids as IR Standards for ISOPHOT Asteroids as far-infrared photometric standards for ISOPHOT T G Mueller J S V Lagerros Astron. Astrophys. 338 340 1998 1998A&A...338..340M II/190 : IRAS Minor Planet Survey (IMPS) (Tedesco 1992) http://cadcwww.dao.nrc.ca/jcmt : The JCMT archiveAltenhoff W.J., Baars J.W.M., Schrami J.B. et al. 1996A&A...309..953A Lebofsky L.A., Sykes M.V., Tedesco E.F. et al., 1986Icar...68..239L Mueller, T., 1997, Ph.D. thesis, Ruprecht-Karls-Universitat, Heidelberg Minor planets Polarization Spectra, infrared infrared: solar system minor planets, asteroids radiation mechanisms: thermal Thermal emission observations of 10 selected asteroids. Mid- and far-IR data compiled from a number of sources into uniform database. The table consists of 678 individual observations, ranging from 7 to 2000 microns. Inband fluxes have been converted to monochromatic flux densities. Asteroids are used as far-IR calibrators for the imaging photopolarimeter ISOPHOT on board the Infrared Space Observatory ISO. For the 10 selected objects we compiled a large uniform database of 678 individual observations, ranging from 7-2000{mu}m. Applying a new thermophysical model to the observations we derived thermal properties of the selected asteroids, based on spin-vector solutions, direct size measurements and the HG-magnitude system. Our investigations indicate very rough surfaces, reflected in the beaming effect, and very low levels of heat conduction, expressed in thermal inertias between 5 and 25J/m^2^/s^0.5^/K. Due to scattering processes in the porous regolith, the emissivity varies significantly with wavelength. In case of Vesta we find emissivities as low as 0.6 in the far-IR/submillimetre region. By entering the combined results into the thermophysical model we defined new photometric standards for the far-IR. The absolute accuracy for thermal flux or lightcurve predictions is 5-10% for the first category objects and 10-20% for the secondaries. The methods and procedures discussed here are included in the first update of the ISOPHOT calibration in 1998.
Thermal emission observations of 10 selected asteroids Asteroid Asteroid number. See Note number=1 The IAU designation (number and name) 1 Ceres 2 Pallas 3 Juno 4 Vesta 10 Hygiea 54 Alexandra 65 Cybele 106 Dione 313 Chaldaea 532 Herculina --- JD Julian Date d lambda Wavelength um flux Monochromatic flux Jy e_flux Flux error Jy Inst Telescope and instrument. See Note number=2 Telescope and instrument: HHT: Heinrich-Hertz-Telescope IRAS: Infrared Astronomical Satellite IRTF: Infrared Telescope Facility ISO/ISOPHOT: Infrared Space Observatory / Imaging-Photopolarimeter JCMT/UKT14: James Clerk Maxwell Telescope / United Kingdom Telescope, Cryostat No. 14-Bolometer UKIRT/MAX: United Kingdom Infrared Telescope / Mid-Infrared Array eXpandable-Camera --- Johan Lagerros Uppsala Astronomical Observatory 1998 Sep 08 Johan Lagerros <jl@astro.uu.se> J_A+A_338_340.xml Field #3 of the Palomar-Groningen survey. II. Near-infrared photometry of semiregular variables. J/A+A/338/581 J/A+A/338/581 Field 3 Palomar-Groningen survey. II. Field #3 of the Palomar-Groningen survey. II. Near-infrared photometry of semiregular variables. M Schultheis Y K Ng J Hron F Kerschbaum Astron. Astrophys. 338 581 1998 1998A&A...338..581S J/A+AS/123/115 : Field 3 of the Palomar-Groningen Survey. I. (Ng+ 1997) Wesselink Th.J.H., 1987, Ph.D. thesis, Catholic University Nijmegen, the Netherlands Photometry, infrared Stars, variable Galaxy: center stars: AGB and post-AGB stars: evolution Near-infrared photometry (JHKL'M) was obtained for 78 semiregular variables (SRVs) in field #3 of the Palomar-Groningen survey (PG3, l=0{deg}, b=-10{deg}). Together with a sample of Miras in this field a comparison is made with a sample of field SRVs and Miras. The PG3 SRVs form a sequence (period-luminosity & period-colour) with the PG3 Miras, in which the SRVs are the short period extension to the Miras. The field and PG3 Miras follow the same P/(J-K)_0_ relation, while this is not the case for the field and PG3 SRVs. Both the PG3 SRVs and Miras follow the Sgr I period-luminosity relation adopted from Glass et al. (1995MNRAS.273..383G). They are likely pulsating in the fundamental mode and have metallicities spanning the range from intermediate to approximately solar.
Near-infrared photometry for the stars in field #3 of the Palomar-Groningen Variable Star Survey (Plaut, 1971A&AS....4...75P). Name Stellar identifier, from Wesselink (1987) --- VarType Variable type from Plaut (1971A&AS....4...75P) --- Jmag J magnitude number=1 Typical errors are ~0.02mag in JHK, ~0.1mag in L' and >0.2mag in M. mag Hmag H magnitude number=1 Typical errors are ~0.02mag in JHK, ~0.1mag in L' and >0.2mag in M. mag Kmag K magnitude number=1 Typical errors are ~0.02mag in JHK, ~0.1mag in L' and >0.2mag in M. mag L'mag L' magnitude number=1 Typical errors are ~0.02mag in JHK, ~0.1mag in L' and >0.2mag in M. mag Mmag M magnitude number=1 Typical errors are ~0.02mag in JHK, ~0.1mag in L' and >0.2mag in M. mag Run Observing run identifier number=2 1: 28 Jul - 2 Aug 1990, Observer: Ng 2: 21 May - 3 Jun 1991, Observer: Brown 3: 20 - 29 Aug 1991 Observer: Ng 4: 16 - 21 Jun 1992, Observers: Ng & Schultheis 5: 29 Jun - 3 Jul 1993, Observers: Ng & Schultheis --- Per Period determined by Wesselink (1987) if available d q_Per Quality flag related with the period and the identification of the star number=3 0: no doubt about the determined period and classification 1: classification is correct but alternative period is possible 2: period determination is correct but the classification is doubtful 3: both period determination and classification are unreliable --- Patricia Bauer CDS 1998 Sep 11 Mathias Schultheis <schulthe@iap.fr> J_A+A_338_581.xml Updating the {sigma}-T relationship for galaxy clusters J/A+A/338/813 J/A+A/338/813 Galaxy clusters {sigma}-T relationship Updating the {sigma}-T relationship for galaxy clusters X -P Wu L -Z Fang W Xu Astron. Astrophys. 338 813 1998 1998A&A...338..813W Clusters, galaxy Velocity dispersion galaxies: clusters: general X-rays: galaxies This is a sample of 149 galaxy clusters for which both the X-ray determined temperature T of the intracluster gas and the optical measured velocity dispersion {sigma} of the cluster galaxies have been available.
Cluster Sample Cluster Cluster name --- z Redshift --- T Temperature of the X-ray intracluster gas keV E_T Error in T (upper limit) keV e_T Error in T (lower limit) keV sigma Velicoty dispersion of the cluster galaxies km/s E_sigma Error in sigma (upper limit) km/s e_sigma Error in sigma (lower limit) km/s beta {beta} spectral index --- e_beta rms uncertainty on beta --- table1.ps PostScript version of table1.dat table1.tex LaTeX version of table1.dat Patricia Bauer CDS 1998 Aug 14 Xiang-Ping Wu <Xiang-Ping.Wu@gin.obspm.fr>, <wu@time.physics.arizona.edu> J_A+A_338_813.xml The evolution of helium white dwarfs. I. The companion of the millisecond pulsar PSR J1012+5307 J/A+A/339/123 J/A+A/339/123 PSR J1012+5307 evolutionary tracks The evolution of helium white dwarfs. I. The companion of the millisecond pulsar PSR J1012+5307 T Driebe D Schoenberner T Bloeckera F Herwig Astron. Astrophys. 339 123 1998 1998A&A...339..123D Models, evolutionary Pulsars Stars, dwarfs pulsars: individual (PSR J1012+5307) stars: evolution stars: interiors white dwarfs We present a set of evolutionary tracks for white dwarfs with helium cores in the mass range from 0.179 to 0.414M_{sun}_. The tracks are based on a 1M_{sun}_ model sequence extending from the pre-main sequence stage up to the tip of the red-giant branch. Applying large mass loss rates at appropriate positions forced the models to move off the giant branch.The further evolution was then followed across the Hertzsprung-Russell diagram and down the cooling branch.
PSR J1012+5307 PSR J1012+53 10 12 33.5 +53 07 03
Evolutionary tracks for Mfinal=0.179M_sun_ Evolutionary tracks for Mfinal=0.195M_sun_ Evolutionary tracks for Mfinal=0.234M_sun_ Evolutionary tracks for Mfinal=0.259M_sun_ Evolutionary tracks for Mfinal=0.300M_sun_ Evolutionary tracks for Mfinal=0.331M_sun_ Evolutionary tracks for Mfinal=0.414M_sun_ Mfinal Final mass solMass Age Cooling Age yr log(Teff) Effective temperature [K] log(L) Luminosity [solLum] log(g) Surface gravity [cm/s2] R Radius solRad log(Tc) Central temperature [K] Log(rhoc) Central density [g/cm3] Lg Gravothermal luminosity solLum Lh Hydrogen luminosity solLum Mh Mass of the hydrogen exhausted core solMass Patricia Bauer CDS 1998 Oct 08 Thomas Driebe <driebe@speckle.mpifr-bonn.mpg.de> J_A+A_339_123.xml Line identifications and preliminary abundances from the red spectrum of HD 101065 (Przybylski's star) J/A+A/339/165 J/A+A/339/165 The red spectrum of HD 101065 Line identifications and preliminary abundances from the red spectrum of HD 101065 (Przybylski's star) C R Cowley G Mathys Astron. Astrophys. 339 165 1998 1998A&A...339..165C Abundances, peculiar Spectra, red Stars, peculiar stars: abundances stars: chemically peculiar stars: individual (HD 101065) stars: magnetic fields Wavelength list for Przybylski's star (a rapidly rotation Ap star) including a measurement of the line depths.
HD 101065 Przybylski's star 11 37 37.2 -46 42 37
Wavelength list for Przybylski's star Lambda Measured wavelength 0.1nm Int Measured central intensity number=1 Central depth of the line, as measured from a convolved and Fourier filtered spectrum (1.00 corresponds to the continuum level). --- Strength Line strength number=2 Estimate of the line strength on an arbitrary scale, derived from the measured line depth. Intensities of lines in the wing of H{alpha} are eye estimates, and not computed from the line depths. They are given with colons --- n_Strength : when eye estimates --- Id1 First identification number=3 Up to 4 possible contributing transitions are identified for the measured lines. The fractional part of the laboratory wavelength of the transition is given, followed by spectrum (e.g. Nd II). For most of the lanthanide spectra, the parenthesized number following the spectrum is the intensity from Meggers, Corliss, and Scribner (NBS Monog. 145, 1975). Iron-group spectra are typically followed by Multiplet numbers (e.g. Fe I-15 is a line from Multiplet 15). Energy levels are sometimes given for third spectra of the lanthanides. These are from Martin, Zalubas, and Hagan (NSRDS-NBS 60, 1978), or unpublished material provided to CRC by Hannah Crosswhite. Lines lacking energy-level classifications are designated "uncl." --- Id2 Second identification number=3 Up to 4 possible contributing transitions are identified for the measured lines. The fractional part of the laboratory wavelength of the transition is given, followed by spectrum (e.g. Nd II). For most of the lanthanide spectra, the parenthesized number following the spectrum is the intensity from Meggers, Corliss, and Scribner (NBS Monog. 145, 1975). Iron-group spectra are typically followed by Multiplet numbers (e.g. Fe I-15 is a line from Multiplet 15). Energy levels are sometimes given for third spectra of the lanthanides. These are from Martin, Zalubas, and Hagan (NSRDS-NBS 60, 1978), or unpublished material provided to CRC by Hannah Crosswhite. Lines lacking energy-level classifications are designated "uncl." --- Id3 Third identification number=3 Up to 4 possible contributing transitions are identified for the measured lines. The fractional part of the laboratory wavelength of the transition is given, followed by spectrum (e.g. Nd II). For most of the lanthanide spectra, the parenthesized number following the spectrum is the intensity from Meggers, Corliss, and Scribner (NBS Monog. 145, 1975). Iron-group spectra are typically followed by Multiplet numbers (e.g. Fe I-15 is a line from Multiplet 15). Energy levels are sometimes given for third spectra of the lanthanides. These are from Martin, Zalubas, and Hagan (NSRDS-NBS 60, 1978), or unpublished material provided to CRC by Hannah Crosswhite. Lines lacking energy-level classifications are designated "uncl." --- Id4 Fourth identification number=3 Up to 4 possible contributing transitions are identified for the measured lines. The fractional part of the laboratory wavelength of the transition is given, followed by spectrum (e.g. Nd II). For most of the lanthanide spectra, the parenthesized number following the spectrum is the intensity from Meggers, Corliss, and Scribner (NBS Monog. 145, 1975). Iron-group spectra are typically followed by Multiplet numbers (e.g. Fe I-15 is a line from Multiplet 15). Energy levels are sometimes given for third spectra of the lanthanides. These are from Martin, Zalubas, and Hagan (NSRDS-NBS 60, 1978), or unpublished material provided to CRC by Hannah Crosswhite. Lines lacking energy-level classifications are designated "uncl." --- G. Mathys (ESO, Santiago, Chile), Patricia Bauer CDS 1998 Sep 28 Gautier Mathys <gmathys@eso.org> J_A+A_339_165.xml Bright galaxies from WENSS. I The minisurvey J/A+A/339/34 J/A+A/339/34 Bright galaxies from the WENSS minisurvey Bright galaxies from WENSS. I The minisurvey H R de Ruiter P Parma G M Stirpe I Perez-Fournon I Gonzalez-Serrano R B Rengelink M N Bremer Astron. Astrophys. 339 34 1998 1998A&A...339...34D J/A+AS/124/259/ : Westerbork Northern Sky Survey I. (Rengelink+ 1997) Galaxies, photometry Radio sources Redshifts galaxies: distances and redshifts radio continuum: galaxies A search for bright galaxies associated with radio sources from the Westerbork Northern Sky Survey (WENSS) minisurvey has been carried out. A galaxy counterpart was found for 402 of almost 10,000 radio sources. Of these a radio and optically complete sample, with a flux density limit at 325MHz of 30mJy and a limiting red magnitude of 16, can be constructed, which contains 119 galaxies. This paper is the first step of a more general study, in which we aim to derive a bright galaxy sample from the entire WENSS survey (which is now available in the public domain) and thus to construct practically definitive local radio luminosity functions of elliptical and spiral galaxies. We briefly describe the WENSS minisurvey, and the steps that are needed for the optical identification of its radio sources. Due to the large numbers of sources involved (over 200,000) completely automated procedures are obviously needed and we discuss these in some detail. It is shown that with modern utilities projects as described here have become quite feasible. Some results (e.g. a preliminary determination of the local radio luminosity function) are presented.
The minisurvey bright galaxy sample Seq Running number from minisurvey --- IAUname IAU name of radio source number=1 Names in the form WNBhhmm+ddmm; WN hhmm+ddmm in Simbad --- Speak Peak flux density of radio source mJy Stot Total flux density of radio source mJy Oname Optical catalogue name number=2 ZWG nnn.0nn = Z nnn - nn in Simbad 7 ZW nnn = ZW VII nnn in Simbad --- Otype Galaxy type --- Rmag Red magnitude of the galaxy mag z Redshift of the galaxy --- n_z *: new redshift --- DRA Right ascension difference (radio minus optical) arcsec DDE Declination difference (radio minus optical) arcsec SI Spectral index (325-1400MHz) --- Patricia Bauer CDS 1998 Aug 14 Hans de Ruiter <deruiter@kennet.bo.astro.it> J_A+A_339_34.xml Red giants in open clusters: VIII. NGC 752 J/A+A/339/423 J/A+A/339/423 Velocities of red giants in NGC 752 Red giants in open clusters: VIII. NGC 752 J -C Mermilliod R D Mathieu D W Latham M Mayor Astron. Astrophys. 339 423 1998 1998A&A...339..423M J/A+A/299/53 : Red giants in NGC 3680 and IC 4651 (Mermilliod+, 1995) J/A+A/307/80 : Velocities of red giants in NGC 2099 (Mermilliod+ 1996) J/A+A/319/481 : Radial velocities of 10 spectros. binaries (Mermilliod+ 1997) J/A+A/324/91 : Melotte 71 red giants radial velocities (Mermilliod+ 1997) Mermilliod & Mayor, Paper I. 1989A&A...219..125M Mermilliod et al., Paper II. 1989A&AS...79...11M Mermilliod & Mayor, Paper III. 1990A&A...237...61M Mermilliod et al., Paper IV. 1995A&A...299...53M, Cat. <J/A+A/299/53> Mermilliod et al., Paper V. 1996A&A...307...80M, Cat. <J/A+A/307/80> Mermilliod et al., Paper VI. 1997A&A...319..481M, Cat. <J/A+A/319/481> Mermilliod et al., Paper VII. 1997A&A...324...91M, Cat. <J/A+A/324/91> Clusters, open Radial velocities Stars, giant binaries: spectroscopic Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 752) techniques: radial velocities The results of an 18-year radial-velocity survey of 30 red giants in the field of the open cluster NGC 752 are presented. The membership of 15 stars is confirmed. Four spectroscopic binaries have been discovered among the members and three orbits have been determined for H75, 110 and 208, with periods of 3321, 127 and 5276 days respectively. The binary frequency (27%) is normal. A search for additional members in a wide surrounding area (2{deg}) yielded two possible new members: both are clump red giant candidates. The red giant distribution in the colour-magnitude diagram is somewhat unusual, with a clump containing 8 stars and a second, fainter feature extending to the blue, defined by 3 or 4 stars, which is not accounted for by theoretical isochrones.
List of stars StID Star number denomination, as in tables 4 --- RAh Right Ascension J2000 (hours) number=1 data extracted from SIMBAD h RAm Right Ascension J2000 (minutes) number=1 data extracted from SIMBAD min RAs Right Ascension J2000 (seconds) number=1 data extracted from SIMBAD s DE- Declination J2000 (sign) number=1 data extracted from SIMBAD --- DEd Declination J2000 (degrees) number=1 data extracted from SIMBAD deg DEm Declination J2000 (minutes) number=1 data extracted from SIMBAD arcmin DEs Declination J2000 (seconds) number=1 data extracted from SIMBAD arcsec OtherNames Other designations --- CORAVEL radial velocity data CfA radial velocity data StID Star number denomination number=1 The numbering system used for NGC 752 is from: H: Heinemann K. 1926AN....227..193H, NGC 752 NNN in Simbad J: Junkvist S. 1931, Medd. Astron. Obs. Upsala no 52 N: concerning 3 stars: N1367 = Platais 1263 (Cl* NGC 752 PLA 1263 in Simbad) = Ebb. A3 (Cl* NGC 752 EBBI A3 in Simbad) N1175 = Platais 212 (Cl* NGC 752 PLA 212 in Simbad) N2054 = Platais 172 (Cl* NGC 752 PLA 172 in Simbad) --- HJD Heliocentric Julian Date d RV Radial velocity km/s e_RV Error on the radial velocity km/s Patricia Bauer CDS 1998 Sep 22 Jean-Claude Mermilliod <Jean-Claude.Mermilliod@obs.unige.ch> J_A+A_339_423.xml Towards a fundamental calibration of stellar parameters of A, F, G, K dwarfs and giants J/A+A/339/858 J/A+A/339/858 Calibration of stellar parameters Towards a fundamental calibration of stellar parameters of A, F, G, K dwarfs and giants G P Di Benedetto Astron. Astrophys. 339 858 1998 1998A&A...339..858D I/196 : Hipparcos Input Catalogue, Version 2 (Turon+ 1993) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Effective temperatures Parallaxes, trigonometric Photometry, infrared Stars, dwarfs Stars, giant stars: atmospheres stars: fundamental parameters The results of calibration of the surface brightness, bolometric flux and effective temperature scales are presented for 537 dwarfs and giants selected as standards for the Infrared Space Observatory (ISO). Individual temperatures with small model-dependent corrections are derived at the target accuracy of 1%. The comparison with semiempirical values achieved by the Infrared Flux Method (IRFM) shows consistent results within the 1% level for F, G and K stars, but not for A-type stars.
Observational photometry, Hipparcos parallaxes, total fluxes, intrinsic near-infrared colours on the Johnson scale and effective temperatures of the ISO standard stars (Northern Hemisphere) Observational photometry, Hipparcos parallaxes, total fluxes, intrinsic near-infrared colours on the Johnson scale and effective temperatures of the ISO standard stars (Southern Hemisphere) HIP Hipparcos Input Catalogue (Cat. <I/239>) number --- HR Bright Star (Cat. <V/50>) number --- SpType Spectral Type --- Vmag Magnitude at 0.55 microns mag Kmag TCS or ESO K magnitude at 2.19 microns number=1 TCS magnitude system (Hammersley, to be published) ESO magnitude system (van der Bliek, 1996, Cat. <J/A+AS/119/547>) mag Plx Parallax from Hipparcos (Cat. <I/239>) mas e_Plx Parallax error mas F(BOL) Bolometric flux W/m2 Note See Note number=2 * Data omitted from the fits --- (V-K)0 Intrinsic near-infrared colour mag Teff Effective temperature K Patricia Bauer CDS 1998 Nov 09 Paolo Di Benedetto <pdibene@ifctr.mi.cnr.it> J_A+A_339_858.xml On the determination of the solar iron abundance using Fe II lines J/A+A/340/300 J/A+A/340/300 Fe II oscillator strengths On the determination of the solar iron abundance using Fe II lines A J J Raassen P H M Uylings Astron. Astrophys. 340 300 1998 1998A&A...340..300R J/A+AS/125/539 : Mn III position probabilities (Uylings+ 1997) J/A+AS/130/541 : Co II oscillator strengths (Raassen+ 1998) Atomic physics atomic data Sun: abundances A sample of the agreement between experiment (recent experimental log(gf) values) and our method (orthogonal operator technique) is shown in table 1. The experimental data are taken from the critical compilation by Giridhar and Ferro (1995RMxAA..31...23G) using data from Kroll and Kock (1987A&AS...67..225K), and from most recent data by Bergeson et al. (1996ApJ...464.1044B). Eight lines in this table are indicated by * in front of the orthogonal log(gf) value: for these lines the difference between experimental value and our calculated value is >=0.2.
Comparison of recent experimental log(gf) values and values obtained by means of the orthogonal operator technique Lambda Wavelength 0.1nm log(gf)1 Oscillateur strength, Giridhar and Ferro, 1995RMxAA..31...23G --- log(gf)2 Oscillateur strength, Bergeson et al. 1996ApJ...464.1044B --- f_log(gf)2 indication large difference --- log(gf)3 Oscillateur strength, This work --- Jf J-value final state --- Ef Energy value final state cm-1 Lf Leading term final state --- Ji J-value initial state --- Ei Energy value initial state cm-1 Li Leading term initial state --- Patricia Bauer CDS 1998 Nov 16 P. Uylings <uylings@phys.uva.nl> J_A+A_340_300.xml Polarization properties of a sample of broad absorption line and gravitationally lensed quasars J/A+A/340/371 J/A+A/340/371 Quasar polarization Polarization properties of a sample of broad absorption line and gravitationally lensed quasars D Hutsemekers H Lamy M Remy Astron. Astrophys. 340 371 1998 1998A&A...340..371H J/A+A/332/410 : Quasar polarization (Hutsemekers 1998) Polarization QSOs gravitaional lensing polarization quasars: absorption lines quasars: general Table 2 contains optical (V) polarimetric measurements for 42 optically selected QSOs including 29 broad absorption line QSOs. Table 3 contains a series of spectral indices characterizing the broad absorption line QSOs.
Polarimetric results Name Quasar name (from 1950 position) --- z Redshift --- Type Object type number=1 Object Type: 1: non-BAL QSOs + one intermediate object 2: HIBAL QSOs 3: Strong LIBAL QSOs 4: Weak LIBAL QSOs 5: Marginal LIBAL QSOs 6: unclassified BAL QSOs --- Note 1: objects identified as true or possible gravitationally lensed QSOs --- Q Normalized Stokes parameter Q % e_Q Uncertainty of Normalized Stokes parameter Q % U Normalized Stokes parameter U % e_U Uncertainty of Normalized Stokes parameter U % Pol Polarization degree % e_Pol Uncertainty of polarization degree % Pold Debiased polarization degree % Poli Interstellar polarization % PA Polarization position angle deg e_PA Uncertainty of polarization position angle deg BAL QSO spectral characteristics Name Quasar name (from 1950 position) --- Type Object type number=1 Object Type: 1: non-BAL QSOs + one intermediate object 2: HIBAL QSOs 3: Strong LIBAL QSOs 4: Weak LIBAL QSOs 5: Marginal LIBAL QSOs 6: unclassified BAL QSOs --- Note 1: objects identified as true or possible gravitationally lensed QSOs --- BI Balnicity index number=2 The balnicity index is a modified velocity equivalent width of the C IV broad absorption line. See Weymann et al., 1991ApJ...373...23W. km/s DI Detachment index number=3 The detachment index is the degree of detachment of the absorption line relative to the emission one. See Weymann et al., 1991ApJ...373...23W. --- HWHM(CIV) CIV Half Width at Half Maximum km/s HWHM(CIII) CIII] Half Width at Half Maximum km/s EW(CIV) CIV equivalent width 0.1nm EW(CIII) CIII] equivalent width 0.1nm EW(FeII2400) FeII 2400 equivalent width 0.1nm EW(FeII2070) FeII 2070 equivalent width 0.1nm Bcont Continuum slope B --- Rcont Continuum slope R --- Hutsemekers Liege University Patricia Bauer CDS 1998 Oct 13 Damien Hutsemekers <hutsemek@astro.ulg.ac.be> J_A+A_340_371.xml Visual binary orbits and masses post Hipparcos J/A+A/341/121 J/A+A/341/121 Visual binary orbits and masses Visual binary orbits and masses post Hipparcos S Soederhjelm Astron. Astrophys. 341 121 1999 1999A&A...341..121S I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Binaries, orbits Parallaxes, trigonometric Stars, double and multiple Stars, masses astrometry binaries: general binaries: visual catalogs stars: fundamental parameters The paper gives orbits and masses for some 200 nearby visual binaries, as derived from combining ground-based and Hipparcos data. Table 6 gives identifications and notes, and points to the detailed data in Table 1 (short-P systems with mass-ratio from the Hipparcos observations), Table 3 (mass-uncertainty below 10%) or Table 4 (mass-uncertainty above 10%).
Astrometrically determined mass-ratios with improved orbital elements and parallaxes HIP HIP (Cat. <I/239>) identifier --- n_HIP b when two solutions for the object --- Hp1 Primary Hp magnitude mag m2-m1 Magnitude difference (secondary-primary) mag M2/M1 Mass-ratio (secondary/primary) --- e_M2/M1 Mean error for M2/M1 --- plx Parallax in present solutions mas e_plx Mean error for plx mas plx(HIP) Parallax in HIP (Cat. <I/239>) mas e_plx(HIP) Mean error for plx(HIP) mas eps Total mass-uncertainty % eps(p) Mass-uncertainty due to parallax % eps(o) Mass-uncertainty due to orbit % Msum Mass-sum solMass Note Note number=1 m: previously known or suspected spectroscopic subsystem n: note in notes.dat file g: giant spectrum --- Per Orbit period yr T Epoch of periastron yr a Orbit semi-major axis arcsec e Eccentricity --- i Orbit inclination deg omega Orbit argument of periastron deg OMEGA Orbit PA of node deg The most accurate mass-sums and orbital elements for the systems without astrometric mass-ratio Data as in table3.dat, but for the systems with estimated mass-uncertainty above 10%. HIP HIP (Cat. <I/239>) identifier --- m_HIP Multiplicity index on HIP (71683/1) --- n_HIP b when two solutions for the object --- Hp1 Primary Hp magnitude mag l_m2-m1 Limit flag on m2-m1 --- m2-m1 Magnitude difference (secondary-primary) mag u_m2-m1 Uncertainty flag on m2-m1 --- V-I Combined (primary+secondary) V-I color mag plx Parallax in present solutions mas e_plx Mean error for plx mas plx(HIP) Parallax in HIP (Cat. <I/239>) mas e_plx(HIP) Mean error for plx(HIP) mas u_plx(HIP) Uncertainty flag on plx(HIP) --- MHp1 Absolute magnitude of primary mag eps Total mass-uncertainty % eps(p) Mass-uncertainty due to parallax % eps(o) Mass-uncertainty due to orbit % Msum Mass-sum solMass q Photometric mass-ratio --- u_q Uncertainty flag on q --- Note Note number=1 m: spectroscopic subsystem g: non-MS component n: note in notes.dat file --- Per Orbit period yr u_Per Uncertainty flag on Per --- T Epoch of periastron yr a Orbit semi-major axis arcsec u_a Uncertainty flag on a --- e Eccentricity --- i Orbit inclination deg omega Orbit argument of periastron deg OMEGA Orbit PA of node deg Cross-identifications for the systems mentioned in this paper Name Bayer/Flamsteed designation --- HIP HIP (Cat. <I/239>) identifier --- CCDM CCDM (Cat. <I/211>) identifier (hhmmm+-ddmm) --- u_CCDM Uncertainty flag on CCDM --- ADS ADS identifier --- Disc Discoverer designation --- Tab pointer to Table 1,3,4 number=1 0 indicates that the object is not in tables 1, 3 or 4. --- Note *: Note in notes.dat file --- Individual notes HIP HIP (Cat. <I/239>) identifier --- Note Text of the note --- Patricia Bauer CDS 1998 Dec 03 Staffan Soderhjelm <staffan@astro.lu.se> J_A+A_341_121.xml A search for star formation in the translucent clouds MBM 7 and MBM 55 J/A+A/341/163 J/A+A/341/163 MBM 7 and MBM 55 X-ray sources A search for star formation in the translucent clouds MBM 7 and MBM 55 T Hearty L Magnani J -P Caillault R Neuhaeuser J H M M Schmitt J Stauffer Astron. Astrophys. 341 163 1999 1999A&A...341..163H IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) IX/11 : ROSAT Source Catalog (Voges+ 1994) X-ray sources ISM: clouds stars: formation The star formation capability of two molecular clouds at high galactic latitude (|b|>30{deg}) is investigated. Possible pre-main sequence stars in and around the translucent clouds MBM7 and MBM55 have been identified via their X-ray emission by inspecting ROSAT All-Sky Survey observations of the clouds and environs and ROSAT pointed observations of the high-density cores within the clouds. Follow-up optical spectroscopy of the stellar X-ray sources with V<=15.5mag was conducted with the 1.5-m Fred Lawrence Whipple Observatory telescope to identify standard signatures of pre-main sequence stars (LiI {lambda}6708{AA} absorption and H{alpha} emission). We found 11 stars which have lithium equivalent widths, W(Li), above our detection threshold. Three of the stars with lithium also have weak H{alpha} emission. Relative ages for the stars with lithium are estimated by their position on an W(Li) vs. T_eff_ diagram. A calibration derived from data for several clusters with known ages indicates that the stars are older than the translucent high-latitude clouds. This conclusion is supported by a comparison with theoretical evolutionary tracks of the stars from our sample for which we have distance measurements from Hipparcos. We find it is unlikely that any of the X-ray active, lithium-rich stars we identified have formed in the clouds in question. Theoretical and observational arguments support this conclusion and render unlikely the possibility that low-extinction translucent clouds are the sites of star formation.
X-ray identified sources with probable stellar optical counterparts Note Source localisation number=1 A: MBM 7 RASS stars B: MBM 7 ROSAT pointed observation stars C: MBM 55 RASS stars D: MBM 55 ROSAT pointed observation stars --- RX RXJ name of the X-ray source --- m_RX Multiplicity index on Name --- n_RX *: This source was detected in both the RASS and ROSAT pointed observations. --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec ML Maximum likelihood of existence --- CountRate Broad band (0.1-2.0 keV) count rate ct/s e_CountRate rms uncertainty on CountRate ct/s l_HR1 limit flag on HR1 --- HR1 Hardness ratio 1 --- e_HR1 rms uncertainty on HR1 --- l_HR2 Limit flag on HR2 --- HR2 Hardness ratio 2 --- e_HR2 rms uncertainty on HR2 --- Vmag V magnitude mag n_Vmag Uncertainty flag or note number=2 b: The optical source is just outside of the 40" error circle. --- log(fx/fv) X-ray to optical flux ratio --- SpType Spectral type of the optical counterpart --- EWHa H{alpha} equivalent width number=3 Negative values of W(H{alpha}) indicate emission lines. The errors in equivalent width measurements are ~0.06{AA}. 0.1nm n_EWHa When interval --- EWHa2 Second H{alpha} equivalent width value when interval 0.1nm EWLi Li (6708{AA}) equivalent width number=3 Negative values of W(H{alpha}) indicate emission lines. The errors in equivalent width measurements are ~0.06{AA}. 01.nm Com Comment number=4 1: The H{alpha} and lithium measurements listed in the table are from Frasca & Catalano (1994A&A...284..883F) and Fekel & Balachandran (1993ApJ...403..708F), respectively. 2: This star is listed as a BY Dra candidate in the EEMSS (Stocke et al., 1991ApJS...76..813S). 3: Cutispoto et al. (1996A&AS..115...41C) list this star as a binary with K1/2 IV and F5 V components. It is listed as a G5 in SIMBAD. *: Individual note in notes.dat file --- Individual notes RX RXJ name of the X-ray source --- m_RX Multiplicity index on RXJ --- Note Text of the note --- table3.ps PostScript version of table3 table3.tex LaTeX version of table3 Patricia Bauer CDS 1998 Dec 03 Thomas J. Hearty <thearty@xray.mpe.mpg.de> J_A+A_341_163.xml Brightening of the T Tauri star RY Tau in 1996. Photometry, polarimetry and high resolution spectroscopy J/A+A/341/553 J/A+A/341/553 RY Tau in 1996 Brightening of the T Tauri star RY Tau in 1996. Photometry, polarimetry and high resolution spectroscopy P P Petrov G V Zajtseva Yu S Efimov R Duemmler I V Ilyin I Tuominen V A Shcherbakov Astron. Astrophys. 341 553 1999 1999A&A...341..553P Photometry, UBVRI Polarization Stars, pre-main sequence circumstellar matter stars: individual (RY Tau) stars: pre-main sequence The T Tauri star RY Tau has increased its brightness from V=10.6mag to V=9.6mag in October-November 1996. By February-March 1997, the star has faded again to V=10.8mag. High-resolution echelle spectra of RY Tau were obtained wit h the SOFIN spectrograph at the Nordic Optical Telescope (La Palma, Spain) at lo w and high brightness levels of the star. No significant changes in the photosph eric lines, which are sensitive to temperature and gravity, were noticed. The spectral type of RY Tau is defined as G1-2IV, which in combination with photomet ric data implies A_V_=1.0-1.3mag. Polarimetric patrol of RY Tau during the fadin g of the star showed an increase of its intrinsic polarization from 0.5-1.0% at high brightness to about 2% at low brightness in the V, R and I bands. The flux radiated in H{alpha} and the IR Ca II emission lines remained about the same, in spite of the one magnitude difference in the continuum flux. These results indicate that variable obscuration of the star by circumstellar dust clo uds was responsible for the brightness change of RY Tau, and that the emission l ine source is mostly outside of the obscured region.
RY Tau HD 283571 04 21 57.3 +28 26 37
UBV-photometry of RY Tau in 1965-1997 JD Julian Date d Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag Observed and intrinsic polarization of RY Tau in UBVRI JD Julian Date d band photometric band (U,B,V,R,I) --- mag Brightness in that band mag P(obs) Observed polarization in that band % e_P(obs) Mean error of the observed polarization % PA(obs) Observed position angle of polarization in that band deg e_PA(obs) Mean error of observed position angle deg P(intr) Intrinsic polarization in that band (after correction for interstellar polarization) number=1 correction for interstellar polarization: P(max)=2.84%, PA=26 deg. (lambda(max)=5500{AA}) (see text) % e_P(intr) Mean error of intrinsic polarization % PA(intr) Position angle of intrinsic polarization in that band (after correction for interstellar polarization) deg e_PA(intr) Mean error of position angle of intrinsic polarization deg CDS 1998 Oct 28 Rolf Duemmler <rolf@hiisi.oulu.fi> J_A+A_341_553.xml The NTT SUSI Deep Field. J/A+A/341/641 J/A+A/341/641 NTT SUSI Deep Field The NTT SUSI Deep Field. S Arnouts S D'Odorico S Cristiani S Zaggia A Fontana E Giallongo Astron. Astrophys. 341 641 1999 1999A&A...341..641A Galaxies, photometry cosmology: observations galaxies: evolution galaxies: stellar content large-scale structure of universe This catalog contains BVrI photometry of galaxies in a 5.62arcmin^2^ field 80arcsec south of the high redshift (z=4.7) quasar BR 1202-0725, derived from observations with the direct CCD camera SUSI at the ESO NTT. The formal 5{sigma}magnitude limits (in 2xFWHM apertures) are 26.9, 26.5, 25.9 and 25.3 in B, V, r and I respectively. Reliable colors have been measured for galaxies selected down to r=26. The choice of the optical filters has been optimized to define a robust multicolor selection of galaxies at 3.8<=z<=4.4. The catalogue has been processed with the SExtractor algorithm (Bertin, 1996A&AS..117..393B) and contains 608 objects detected on the image resulting from the sum of the four weighted frames (B, V, r, I) by convolving the reference frame by the PSF and then thresholding it at 1.1 {sigma} of the background r.m.s. For quantitative analysis, border areas with larger noise due to the combination of dithered exposures with shorter integration times should be used with caution.
NTT SUSI Deep Field catalogue NDFa Identification number (NTT Deep Field a) --- Xpos X position pix Ypos Y position pix RAh Right Ascension, equinox 2000 h RAm Right Ascension, equinox 2000 min RAs Right Ascension, equinox 2000 s DE- Declination sign, equinox 2000 --- DEd Declination, equinox 2000 deg DEm Declination, equinox 2000 arcmin DEs Declination, equinox 2000 arcsec Bmag B total magnitude in natural system number=1 The total magnitudes are isophotal magnitudes (at 1{sigma}) if the isophotal area is larger than 2.2arcsec aperture (17 pix) or they are measured inside the 2.2arcsec apertures corrected to 5arcsec by assuming stellar wings. They are in natural photometric systems and galactic absorption has been applied. mag e_Bmag rms uncertainty on Bmag number=2 Objects with computed magnitudes fainter than the expected magnitude limits at 1{sigma} in 2.2arcsec aperture (28.2, 27.7, 27.0, 26.3 in B, V, r, I) have been assigned an upper limit and a value of -1 is entered for the associated error. mag Vmag V total magnitude in natural system number=1 The total magnitudes are isophotal magnitudes (at 1{sigma}) if the isophotal area is larger than 2.2arcsec aperture (17 pix) or they are measured inside the 2.2arcsec apertures corrected to 5arcsec by assuming stellar wings. They are in natural photometric systems and galactic absorption has been applied. mag e_Vmag rms uncertainty on Vmag number=2 Objects with computed magnitudes fainter than the expected magnitude limits at 1{sigma} in 2.2arcsec aperture (28.2, 27.7, 27.0, 26.3 in B, V, r, I) have been assigned an upper limit and a value of -1 is entered for the associated error. mag rmag r total magnitude in natural system number=1 The total magnitudes are isophotal magnitudes (at 1{sigma}) if the isophotal area is larger than 2.2arcsec aperture (17 pix) or they are measured inside the 2.2arcsec apertures corrected to 5arcsec by assuming stellar wings. They are in natural photometric systems and galactic absorption has been applied. mag e_rmag rms uncertainty on rmag number=2 Objects with computed magnitudes fainter than the expected magnitude limits at 1{sigma} in 2.2arcsec aperture (28.2, 27.7, 27.0, 26.3 in B, V, r, I) have been assigned an upper limit and a value of -1 is entered for the associated error. mag Imag I total magnitude in natural system number=1 The total magnitudes are isophotal magnitudes (at 1{sigma}) if the isophotal area is larger than 2.2arcsec aperture (17 pix) or they are measured inside the 2.2arcsec apertures corrected to 5arcsec by assuming stellar wings. They are in natural photometric systems and galactic absorption has been applied. mag e_Imag rms uncertainty on Imag number=2 Objects with computed magnitudes fainter than the expected magnitude limits at 1{sigma} in 2.2arcsec aperture (28.2, 27.7, 27.0, 26.3 in B, V, r, I) have been assigned an upper limit and a value of -1 is entered for the associated error. mag FWHM Full Width Half Maximum number=3 Classifier provided by SExtraxtor applied to the I band, to which corresponds the best PSF. This classifier gives output values in the range 0-1 (0 for galaxies and 1 for stars). pix Flag SExtractor flag --- Class Star/galaxy classifier number=4 Shape parameters in columns FWHM to AREA are given from the I image which has the best seeing. --- a Semi major axis length pix b Semi minor axis length pix Theta Inclination angle deg elong Elongation (a/b) --- e Ellipticity (1-b/a) --- AREA Isophotal area (in pixel) pix B-V B-V colour index in AB system number=5 Colours have been computed by the difference of adaptive apertures for bright objects (isophotal area>180pixels, I<=23) and for the faintest ones inside the 2 arcsec apertures (~15pixels). For these measurements the I frame has been degraded to the worst seeing of the B band. mag e_B-V Quadratic error on B-V number=6 When there is an upper limit, the error is -3.00, -2.00 or -1.00. For example, colour = B-A if B is upper-limit and not A, e_B-A=-1 if A is upper-limit and not B, e_B-A=-2 if B and A are both upper-limits, e_B-A=-3 mag B-R B-R colour index in AB system number=5 Colours have been computed by the difference of adaptive apertures for bright objects (isophotal area>180pixels, I<=23) and for the faintest ones inside the 2 arcsec apertures (~15pixels). For these measurements the I frame has been degraded to the worst seeing of the B band. mag e_B-R Quadratic error on B-R number=6 When there is an upper limit, the error is -3.00, -2.00 or -1.00. For example, colour = B-A if B is upper-limit and not A, e_B-A=-1 if A is upper-limit and not B, e_B-A=-2 if B and A are both upper-limits, e_B-A=-3 mag B-I B-I colour index in AB system number=5 Colours have been computed by the difference of adaptive apertures for bright objects (isophotal area>180pixels, I<=23) and for the faintest ones inside the 2 arcsec apertures (~15pixels). For these measurements the I frame has been degraded to the worst seeing of the B band. mag e_B-I Quadratic error on B-I number=6 When there is an upper limit, the error is -3.00, -2.00 or -1.00. For example, colour = B-A if B is upper-limit and not A, e_B-A=-1 if A is upper-limit and not B, e_B-A=-2 if B and A are both upper-limits, e_B-A=-3 mag V-R V-R colour index in AB system number=5 Colours have been computed by the difference of adaptive apertures for bright objects (isophotal area>180pixels, I<=23) and for the faintest ones inside the 2 arcsec apertures (~15pixels). For these measurements the I frame has been degraded to the worst seeing of the B band. mag e_V-R Quadratic error on V-R number=6 When there is an upper limit, the error is -3.00, -2.00 or -1.00. For example, colour = B-A if B is upper-limit and not A, e_B-A=-1 if A is upper-limit and not B, e_B-A=-2 if B and A are both upper-limits, e_B-A=-3 mag V-I V-I colour index in AB system number=5 Colours have been computed by the difference of adaptive apertures for bright objects (isophotal area>180pixels, I<=23) and for the faintest ones inside the 2 arcsec apertures (~15pixels). For these measurements the I frame has been degraded to the worst seeing of the B band. mag e_V-I Quadratic error on V-I number=6 When there is an upper limit, the error is -3.00, -2.00 or -1.00. For example, colour = B-A if B is upper-limit and not A, e_B-A=-1 if A is upper-limit and not B, e_B-A=-2 if B and A are both upper-limits, e_B-A=-3 mag R-I R-I colour index in AB system number=5 Colours have been computed by the difference of adaptive apertures for bright objects (isophotal area>180pixels, I<=23) and for the faintest ones inside the 2 arcsec apertures (~15pixels). For these measurements the I frame has been degraded to the worst seeing of the B band. mag e_R-I Quadratic error on R-I number=6 When there is an upper limit, the error is -3.00, -2.00 or -1.00. For example, colour = B-A if B is upper-limit and not A, e_B-A=-1 if A is upper-limit and not B, e_B-A=-2 if B and A are both upper-limits, e_B-A=-3 mag Patricia Bauer CDS 1999 Feb 26 UNKNOWN UNKNOWN //www.eso.org/science/ndf/ J_A+A_341_641.xml Chemically consistent evolution of galaxies: Spiral galaxy models compared to DLA systems J/A+A/341/709 J/A+A/341/709 Chemical spiral galaxies models Chemically consistent evolution of galaxies: Spiral galaxy models compared to DLA systems U Lindner U Fritze-von Alvensleben K J Fricke Astron. Astrophys. 341 709 1999 1999A&A...341..709L J/A+AS/123/305 : Yields of intermediate mass stars (van den Hoek+ 1997) Abundances Models, evolutionary galaxies: evolution quasars: absorption lines We have extended our chemical and cosmological galaxy evolution model to calculate the abundance evolution for altogether 16 different elements in spiral galaxies in a chemically consistent way which is a considerable step towards a more realistic galaxy modeling. All observed element abundances in Damped Lyman {alpha} (LDA) systems have been compiled.
SNII yields calculated by Woosley & Weaver (1995ApJS..101..181W) for models A, B and C (see text) and two different metallicities Z=Z_{sun}_ and Z=0.01 Z_{sun}_. Note A: model A; S: SNIa number=1 In the case of Mass=25m_{sun}_ yields calculated from model A for all five different metallicities Z=1, 0.1, 0.01, 10^-4^ and 0Z_{sun}_ are given. SNIa data are from Nomoto et al. (1997Sci...276.1378N) deflagration model W7 --- Z Initial metallicity Sun Mass Stellar mass solMass n_Mass Note on model number=2 *: Model B **: Model C --- H H yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- He He yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- C C yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- N N yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- O O yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Mg Mg yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Al Al yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Si Si yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- S S yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Ar Ar yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Ca Ca yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Fe Fe yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Ni Ni yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Zn Zn yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Cr Cr yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Mn Mn yield number=3 Normalized formed and ejected mass of element integrated over the stellar lifetime --- Meject Total ejected mass number=4 Meject is the total ejected mass as given by Woosley & Weaver (1995ApJS..101..181W). solMass Diff Difference between Meject and the sum of ejecta given in this table for elements H, He, ..., Mn % Stellar yields for various stellar masses and three different initial metallicities Z=1, 0.2 and 0.05Z_{sun}_ from van den Hoek & Groenewegen (1997, Cat. <J/A+AS/123/305>) Mass Stellar mass solMass H1 H yield for Z=1.0 Z_{sun}_ --- H2 H yield for Z=0.2 Z_{sun}_ --- H3 H yield for Z=0.05Z_{sun}_ --- He1 He yield for Z=1.0 Z_{sun}_ --- He2 He yield for Z=0.2 Z_{sun}_ --- He3 He yield for Z=0.05Z_{sun}_ --- C1 C yield for Z=1.0 Z_{sun}_ --- C2 C yield for Z=0.2 Z_{sun}_ --- C3 C yield for Z=0.05Z_{sun}_ --- N1 N yield for Z=1.0 Z_{sun}_ --- N2 N yield for Z=0.2 Z_{sun}_ --- N3 N yield for Z=0.05Z_{sun}_ --- O1 O yield for Z=1.0 Z_{sun}_ --- O2 O yield for Z=0.2 Z_{sun}_ --- O3 O yield for Z=0.05Z_{sun}_ --- Stellar lifetimes for two different initial metallicities. l_Mass Limit flag on mass --- Mass Stellar mass solMass l_Tau1 Limit flag on Tau1 --- Tau1 Stellar lifetime for Z=1.00Z_{sun}_ Gyr Tau2 Stellar lifetime for Z=0.05Z_{sun}_ Gyr SNII remnants of various progenitor masses, five different initial metallicities Z and three explosion models (A, B and C) from Table3 in Woosley & Weaver (1995ApJS..101..181W) Mass Stellar mass solMass n_Mass Note on model number=1 *: Model B **: Model C --- R1 SN II remnant for Z=1.0000Z_{sun}_ solMass R2 SN II remnant for Z=0.1000Z_{sun}_ solMass R3 SN II remnant for Z=0.0100Z_{sun}_ solMass R4 SN II remnant for Z=0.0001Z_{sun}_ solMass R5 SN II remnant for Z=0.0000Z_{sun}_ solMass Remnants for different stellar masses and initial metallicities (Z=1, 0.2 and 0.05Z_{sun}_) from van den Hoek & Groenewegen (1997, Cat. <J/A+AS/123/305>) Mass Mass solMass R1 Remnant for Z=1.0Z_{sun}_ solMass R2 Remnant for Z=0.2Z_{sun}_ solMass R3 Remnant for Z=0.05Z_{sun}_ solMass tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Dec 04 Ulrich Lindner <ulindner@coma.uni-sw.gwdg.de> J_A+A_341_709.xml Structural Properties of s-Cepheid Velocity Curves. Constraining the location of the {omega}_4_=2{omega}_1_ resonance. J/A+A/341/818 J/A+A/341/818 s-Cepheid velocity curves Structural Properties of s-Cepheid Velocity Curves. Constraining the location of the {omega}_4_=2{omega}_1_ resonance. F Kienzle P Moskalik D Bersier F Pont Astron. Astrophys. 341 818 1999 1999A&A...341..818K J/A+AS/108/9 : Cepheids fundamental parameters I. (Bersier+, 1994) J/A+AS/108/25 : Cepeheids fundamental parameters II. (Bersier+, 1994) J/A+A/305/551 : Chemical composition of the s-Cepheids (Andrievsky+, 1996) Krzyt, T., Moskalik, P., Gorynya, et al., 1999, (in preparation) Radial velocities Stars, variable Cepheids stars: oscillations techniques: radial velocities The light curves of the first overtone Pop. I Cepheids (s-Cepheids) show a discontinuity in their {phi}_21_ vs. P diagram, near P=3.2day. This feature, commonly attributed to the 2:1 resonance between the first and the fourth overtones ({omega}_4_~2{omega}_1_), is not reproduced by the hydrodynamical models. With the goal of reexamining the resonance hypothesis, we have obtained new CORAVEL radial velocity curves for 14 overtone Cepheids. Together with 10 objects of Krzyt et al. (1999, in prep.), the combined sample covers the whole range of overtone Cepheid periods. The velocity Fourier parameters display a strong characteristic resonant behavior. In striking contrast to photometric ones, they vary smoothly with the pulsation period and show no jump at 3.2day. The existing radiative hydrodynamical models match the velocity parameters very well. The center of the {omega}_4_=2{omega}_1_ resonance is estimated to occur at Pr=4.58+/-0.04day, i.e. at a period considerably longer than previously assumed (3.2day). We identify two new members of the s-Cepheid group: MY Pup and V440 Per.
Fourier parameters of cepheids STAR Star name according to GCVS --- Period Period d e_Period One sigma error Period d M Number of data points --- N Number of harmonics fitted --- sigma RMS of the residuals km/s A0 Gamma velocity km/s e_A0 One sigma error gamma velocity km/s A1 Amplitude A1 km/s e_A1 One sigma error amplitude A1 km/s R21 Amplitude ratio A2/A1 --- e_R21 One sigma error amplitude ratio R21 --- f21 Phase shift phi2-2*phi1 --- e_f21 One sigma error phase shift f21 --- R31 =-9.999 Amplitude ratio A3/A1 --- e_R31 =-9.999 One sigma error amplitude ratio R31 --- f31 =-9.999 Phase shift phi3-3*phi1 --- e_f31 =-9.999 One sigma error phase shift f31 --- R41 =-9.999 Amplitude ratio A4/A1 --- e_R41 =-9.999 One sigma error amplitude ratio R41 --- f41 =-9.999 Phase shift phi4-4*phi1 --- e_f41 =-9.999 One sigma error phase shift f41 --- R51 =-9.999 Amplitude ratio A5/A1 --- e_R51 =-9.999 One sigma error amplitude ratio R51 --- f51 =-9.999 Phase shift phi5-5*phi1 --- e_f51 =-9.999 One sigma error phase shift f51 --- RAh Right Ascension J2000 (hours) number=1 columns added at CDS, values from SIMBAD data-base. h RAm Right Ascension J2000 (minutes) number=1 columns added at CDS, values from SIMBAD data-base. min RAs Right Ascension J2000 (seconds) number=1 columns added at CDS, values from SIMBAD data-base. s DE- Declination J2000 (sign) number=1 columns added at CDS, values from SIMBAD data-base. --- DEd Declination J2000 (degrees) number=1 columns added at CDS, values from SIMBAD data-base. deg DEm Declination J2000 (minutes) number=1 columns added at CDS, values from SIMBAD data-base. arcmin DEs Declination J2000 (seconds) number=1 columns added at CDS, values from SIMBAD data-base. arcsec Individual CORAVEL velocities STAR Star name according to GCVS --- HJD Heliocentric julian day d RV Radial velocity km/s e_RV One sigma error km/s Patricia Bauer CDS 1998 Oct 23 Francesco Kienzle <Francesco.Kienzle@obs.unige.ch> J_A+A_341_818.xml The ionizing cluster of 30 Doradus. I. Internal reddening from NTT photometry. J/A+A/341/98 J/A+A/341/98 The ionizing cluster of 30 Doradus. I. The ionizing cluster of 30 Doradus. I. Internal reddening from NTT photometry. F Selman J Melnick G Bosch R Terlevich Astron. Astrophys. 341 98 1999 1999A&A...341...98S II/187 : 30 Doradus OB Associations (Parker 1992) J/AJ/107/1054 : 30 Dor region UBV photometry (Malumuth+, 1994) J/ApJ/413/604 : 30 Dor UV and optical photometry (Hill+, 1993) Clusters, open Photometry, UBV dust, extinction Magellanic Clouds open clusters and associations: general stars: early-type stars: luminosity function, mass function UBV profile fitting photometry is presented for 1469 stars within 90arcsec of the center of the ionizing cluster of 30 Doradus (NGC 2070). A value of 0.82+/-0.03 is found for the extinction parameter S=E(U-B)/E(B-V), constant over almost the whole area covered by this research, with some evidence for local variations. Two reddening components can be identified: a smooth and moderate one that increases towards R136, and a clumpy one varying widely across the face of the cluster. The total-to-selective extinction parameter, R_V_= A_V_/E(B-V), is found to be in the range of 3.0 to 3.7, consistent with previous determinations. A new visualization tool, the colour-magnitude stereogram, is introduced and used to argue that: (1) the observations imply mass segregation in a dust filled cluster; (2) that there has been continuous dust formation near the cluster core up to the present; and (3) that an insidious systematic error has plagued previous determinations of IMF slopes. A method to obtain an unbiased estimate of the slope is discussed.
RMC 136 HD 38268 30 Dor 05 38 42.8 -69 06 03 NGC 2070 05 38 42. -69 05 30
UBV photometry of NGC 2070 star members Seq Star number --- xpos X coordinate x is oriented East to West (- --> +) Position of R136: 456.4 (RA=05 38 42.8, DE=-69 06 03 (J2000)) Scale: 0.13 arcsec/pix pix ypos Y coordinate y is oriented South to North (- --> +) Position of R136: 432.3 (RA=05 38 42.8, DE=-69 06 03 (J2000)) Scale: 0.13 arcsec/pix pix P93 Id in Parker's catalogue A -1 in this column indicates no match with the catalogue of Parker (1993AJ....106..560P, Cat. <II/187>). A negative Parker number (smaller than -1) indicates that the star has spectroscopy. --- Vmag Apparent V magnitude mag e_Vmag Error in apparent V magnitude mag Bmag Apparent B magnitude mag e_Bmag Error in apparent B magnitude mag Umag Apparent U magnitude mag e_Umag Error in apparent U magnitude mag Chi2 Chi**2 parameter from IRAF/DAOPHOT II --- Fernando J. Selman ESO Patricia Bauer CDS 1998 Dec 18 Fernando J. Selman <fselman@sc6.sc.eso.org> J_A+A_341_98.xml Proper motions of faint ROSAT WTT stars in the Chamaeleon region. J/A+A/341/L79 J/A+A/341/L79 Proper motions of faint ROSAT WTT stars Proper motions of faint ROSAT WTT stars in the Chamaeleon region. L Terranegra F Morale A Spagna G Massone M G Lattanzi Astron. Astrophys. 341, L79 ??? ??? 1999 1999A+A...341L..79T I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) I/246 : The ACT Reference Catalog (Urban+ 1997) I/146 : Positions and Proper Motions - North (Roeser+, 1988) I/193 : Positions and Proper Motions - South (Bastian+ 1993) J/A+AS/114/109 : Cha X-ray sources + optical identifications (Alcala+ 1995) Proper motions Radio sources Stars, late-type astrometry stars: fundamental parameters stars: kinematics stars: late-type stars: pre-main sequence We present proper motions of 59 stars of the ROSAT All-Sky Survey (RASS) located in direction of the Chamaeleon star forming region (SFR) in the magnitude range B=5.1-17mag. Proper motions of the fainter stars were newly derived utilizing survey Schmidt plates from the GSC~II plate archive and from a set of special plates taken with the ESO Schmidt telescope. The vector point diagram (VPD) indicates that the certified weak emission-line T Tauri (WTT) stars cluster away from the region occupied by the brighter pre-main-sequence stars (PMS) in Cha I. The distance to this new association is estimated at ~100pc, sensibly smaller than the 150pc generally assumed for the SFR. This yields an upper limit of 2km/s for the velocity dispersion of this new kinematic group. The de-reddened CM diagram of the group members suggest the WTT stars are still PMS objects, but older (3-30Myr) and less massive than previous determinations. These revised age estimates, the newly derived group peculiar velocity, and current distance estimates to the Cha~I/II/III complex would favour in-situ formation against that predicted by high velocity cloud models. Finally, based on a redetermination of the peculiar motions of stars and gas, we speculate that the whole SFR originated from the local Orion spur as a result of more classical mechanisms like interactions with the spiral arms.
ROSAT
Proper motions for the 59 RASS stars Name ROSAT all-sky survey source designation Alcala' et al. (1995, Cat. <J/A+AS/114/109>) or catalogue designation --- n_Name Note on Name number=1 *: The proper motion value for CED 110 is from Grasdalen G. (1977IAUC...42...25G), while the values for SAO 256557 and RXJ1225.3-7857 are from the original catalogue and they are in the FK5 system. However the deviation from the Hipparcos system can be considered negligible in this work. KG: Stars belong to the kinematical group (see text). --- CatNo Astrometric catalog designation --- Cat Catalogue name number=2 A = ACT Catalog (Cat. <I/246>) P = PPM Catalog (Cat. <I/146>, <I/193>) H = Hipparcos Catalog (Cat. <I/239>) S = GSC S039 plate --- pmRA Proper motion in right ascension ({mu}RA*cosDE}) mas/yr e_pmRA rms uncertainty on pmRA mas/yr pmDE Proper motion in declination mas/yr e_pmDE rms uncertainty on pmDE mas/yr plx Parallax from Hipparcos catalogue (<I/239>) mas e_plx rms uncertainty on plx mas SpType Spectral Type --- Vmag Stellar V magnitude mag Type Stellar type number=3 PMS: Pre-Main Sequence stars from the high resolution spectroscopy by Covino et al. (1997A&A...328..187C) W: WTTS from low resolution spectroscopy by Alcala' et al. (1995, Cat. <J/A+AS/114/109>) UBS: uncorrelated bright stars by Alcala' et al. (1995, Cat. <J/A+AS/114/109>) CTTS: Classical T Tauri stars Ae/Be: Herbig Ae/Be stars --- Names Other names --- table1.ps PostScript version of table1 table1.tex LaTeX version of table1 Patricia Bauer CDS 1999 Jan 08 Luciano Terranegra <TERRANEGRA@astrna.na.astro.it> J_A+A_341_L79.xml The ESO Slice Project (ESP) galaxy redshift survey: VI. Groups of Galaxies. J/A+A/342/1 J/A+A/342/1 ESO Slice Project. VI. Groups of Galaxies. The ESO Slice Project (ESP) galaxy redshift survey: VI. Groups of Galaxies. M Ramella G Zamorani E Zucca G M Stirpe G Vettolani C Balkowski A Blanchard A Cappi V Cayatte G Chincarini C Collins L Guzzo H MacGillivray D Maccagni S Maurogordato R Merighi M Mignoli A Pisani D Proust R Scaramella Astron. Astrophys. 342 1 1999 1999A&A...342....1R J/A+AS/130/323 : ESO Slice Project (Vettolani+ 1998) Vettolani et al., Paper I. 1997A&A...325..954V Zucca et al., Paper II. 1997A&A...326..477Z Vettolani et al., Paper III. 1998A&AS..130..323V, Cat. <J/A+AS/130/323> Cappi et al., Paper IV. 1998A&A...336..445C Scaramella et al. Paper V. 1998A&A...334..404S Clusters, galaxy Radial velocities Velocity dispersion cosmology: observations galaxies: clusters: general galaxies: distances and redshifts large-scale structure of universe In Table 1 we present our group catalog. For each group we list the ID number (column 1), the number of members (column 2), the coordinates {alpha}_(1950)_ and {delta}_(1950)_ (columns 3 and 4 respectively), the mean radial velocity cz in km/s corrected for Virgo infall and galactic rotation (column 5), and the velocity dispersion {sigma}_cz_ (column 6). We compute the velocity dispersion following the prescription of Ledermann (1984) for an unbiased estimator of the dispersion (see previous section). We also take into account the cosmological expansion of the universe and the measurement errors according to the prescriptions of Danese et al. (1980A&A....82..322D). The errors we associate to the redshifts are those output by the RVSAO cross-correlation procedure multiplied by a factor 1.6. This factor brings the cross-correlation error in rough agreement with the external error estimated from repeated observations (Vettolani et al., 1998, Cat. <J/A+AS/130/323> -- here we do not distinguish between emission and absorption line redshifts).
ESP groups Groups Groups identification number --- Nmem Number of members --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec cz Mean radial velocity km/s l_sigma limit flag on sigma number=1 In the case of 24 groups, the correction of {sigma}_cz_ for the measurement errors leads to a negative value. The error is given as an upper limit to {sigma}_cz_ for these groups. --- sigma Velocity dispersion km/s Nocz Ratio of galaxies that have not a measured redshift to the number of members number=2 Not all galaxies in the region of the sky covered by the ESP survey have a measured redshift. Of the original target list, 444 objects are not observed, and 207 objects have a noisy spectrum, insufficient for a reliable determination of the redshift. Nocz value gives, for each group, the ratio of these objects to the number of members. --- table1.ps PostScript version of table1 table1.tex LaTeX version of table1 Patricia Bauer CDS 1998 Nov 16 Massimo Ramella <ramella@suw003.oat.ts.astro.it> J_A+A_342_1.xml The "angular size - redshift" relation for compact radio structures in quasars and radio galaxies J/A+A/342/378 J/A+A/342/378 6 and 20cm flux densities of radio galaxies The "angular size - redshift" relation for compact radio structures in quasars and radio galaxies L I Gurvits K I Kellermann S Frey Astron. Astrophys. 342 378 1999 1999A&A...342..378G Active gal. nuclei Galaxies, radio QSOs Radio sources Redshifts VLBI cosmology: observations galaxies: active quasars: general radio continuum: galaxies We discuss the "angular size-redshift" relation for compact radio sources distributed over a wide range of redshifts 0.011<=z<=4.72. Our study is based on a sample of 330 5 GHz VLBI contour maps taken from the literature. Unlike extended source samples, the "angular size - redshift" relation for compact radio sources appears consistent with the predictions of standard Friedmann world models with q_0_=~0.5 without the need to consider evolutionary or selection effects due to a "linear size-luminosity" dependence. By confining our analysis to sources having a spectral index, -0.38<={alpha}<=0.18, and a total radio luminosity, Lh^2^>= 10^26^W/Hz (H_0_=100hkm/s/Mpc, q_0_=0.5 used as a numerical example), we are able to restrict the dispersion in the "angular size-redshift" relation. The best fitting regression analysis in the framework of the Friedmann-Robertson-Walker model gives the value of the deceleration parameter q_0_=0.21+/-0.30 if there are no evolutionary or selection effects due to a "linear size-luminosity", "linear size-redshift" or "linear size-spectral index" dependence.
"VLBI angular size - z" for 330 sources IAU IAU name (based on 1950 position) --- Name Alternative name --- z Redshift --- Type Type of the optical counterpart number=1 Q: quasar B: BL Lac object G: radio galaxy (including Seyfert galaxies of all types) --- S6cm Flux density at 6 cm from Gregory et al. (1996) unless otherwise stated. Jy n_S6cm Note on S6cm number=2 f: Spectral index calculated using S_11_=0.61Jy g: Spectral index calculated using S_11_=3.56Jy h: Spectral index calculated using S_75_=5.05Jy i: Spectral index calculated using S_11_=1.10Jy j: Spectral index calculated using S_11_=1.33Jy k: Spectral index calculated using S_11_=0.40Jy l: Spectral index calculated using S_11_=0.56Jy m: Spectral index calculated using S_11_=0.45Jy n: Spectral index calculated using S_75_=0.14Jy o: Spectral index calculated using S_11_=2.74Jy p: Spectral index calculated using S_11_=1.08Jy q: S_6_ and S_20_ values for the compact core component x: Spectral index calculated using S_11_=1.76Jy y: Spectral index calculated using S_11_=1.34Jy --- S20cm Flux density at 20 cm (or alternative) from White and Becker (1992) unless otherwise stated Jy n_S20cm Note on S20cm number=2 f: Spectral index calculated using S_11_=0.61Jy g: Spectral index calculated using S_11_=3.56Jy h: Spectral index calculated using S_75_=5.05Jy i: Spectral index calculated using S_11_=1.10Jy j: Spectral index calculated using S_11_=1.33Jy k: Spectral index calculated using S_11_=0.40Jy l: Spectral index calculated using S_11_=0.56Jy m: Spectral index calculated using S_11_=0.45Jy n: Spectral index calculated using S_75_=0.14Jy o: Spectral index calculated using S_11_=2.74Jy p: Spectral index calculated using S_11_=1.08Jy q: S_6_ and S_20_ values for the compact core component x: Spectral index calculated using S_11_=1.76Jy y: Spectral index calculated using S_11_=1.34Jy --- SI Spectral index --- l_theta Symbol of an upper limit --- theta Angular size mas Struc Structure code number=3 Characteristic angular size (case C) or its upper limit (cases J, L, and S). Radio structure code: C: size between the core and the most distant 2%-component J: upper limit of {theta} along jet direction L: upper limit of {theta} along major axis of the beam S: upper limit of {theta} along minor axis of the beam --- r_z Redshift reference in refs.dat file --- r_S6cm 6cm flux density reference in refs.dat file --- r_S20cm 20cm flux density reference in refs.dat file --- r_VLBI VLBI reference in refs.dat file --- References Ref Reference code --- BibCode BibCode --- Aut Author's name --- Comm Comments ---- table1.tex LaTeX version of table1 table1.ps PostScript version of table1 Patricia Bauer CDS 1998 Dec 04 Leonid Gurvits <lgurvits@jive.nfra.nl> J_A+A_342_378.xml Dark Matter in early-type spiral galaxies: the case of NGC 2179 and of NGC 2775 J/A+A/342/671 J/A+A/342/671 Early-type spiral galaxies kinematics Dark Matter in early-type spiral galaxies: the case of NGC 2179 and of NGC 2775 E M Corsini A Pizzella M Sarzi P Cinzano J C Vega Beltran J G S J Funes F Bertola M Persic P Salucci Astron. Astrophys. 342 671 1999 1999A&A...342..671C VII/72 : Catalog of stellar velocity dispersions. I (Whitmore+ 1985) J/AJ/109/874 : Kinematics of MKW and AWM Poor Clusters (Beers+ 1995) Galaxies, optical Radial velocities Velocity dispersion dark matter galaxies: individual (NGC 2179, NGC 2775) galaxies: kinematics and dynamics galaxies: spiral We present the stellar and ionized-gas velocity curves and velocity-dispersion profiles along the major axis for six early-type spiral galaxies. Two of these galaxies, namely NGC 2179 and NGC 2775, are particularly suited for the study of dark matter halos. Using their luminosity profiles and modeling their stellar and gaseous kinematics, we derive the mass contributions of the luminous and the dark matter to the total potential. In NGC 2179 we find that the data (measured out to about the optical radius R_opt_) unambiguously require the presence of a massive dark halo. For the brighter and bigger object NGC 2775, we can rule out a significant halo contribution at radii R<~0.6R_opt_. Although preliminary, these results agree with the familiar mass distribution trend known for late-type spirals of comparable mass.
IC 724 11 43 34.7 +08 56 30 NGC 2179 06 08 02.1 -21 44 48 NGC 2775 09 10 20.4 +07 02 19 NGC 3281 10 31 52.1 -34 51 13 NGC 4698 12 48 23.0 +08 29 14 NGC 4845 12 58 01.4 +01 34 30
H{alpha} kinematics [NII] ({lambda}6583.4{AA} kinematics [SII] ({lambda}6716.5{AA} kinematics [NII] ({lambda}6548.0{AA} kinematics [SII] ({lambda}6730.8{AA} kinematics Galaxy Galaxy name number=1 halpha.dat, nii6583.dat and sii6716.dat: All galaxies data nii6548.dat: NGC 2775, 3281, 4698 and 4845 data sii6730.dat: NGC 2179, 2775, 3281, 4698, 4845 data --- r Galactocentric distance arcsec HRV Heliocentric radial velocity measured along the major axis km/s e_HRV Heliocentric radial velocity error km/s sigma Velocity dispersion measured along the major axis km/s n Number of rebinned rows --- S/N Signal-to-noise ratio --- Ionized gas kinematics Stellar kinematics Galaxy Galaxy name number=1 gaskin.dat and stelkin.dat: All galaxies data --- r Galactocentric distance arcsec HRV Heliocentric radial velocity km/s e_HRV Heliocentric radial velocity error km/s sigma Velocity dispersion km/s e_sigma Velocity dispersion error km/s Patricia Bauer CDS 1998 Sep 25 Enrico Maria Corsini <corsini@astras.pd.astro.it> J_A+A_342_671.xml Evolution of spectral parameters during a pre-eclipse dip of Her X-1 J/A+A/342/736 J/A+A/342/736 Pre-eclipse dip of Her X-1 Evolution of spectral parameters during a pre-eclipse dip of Her X-1 B Stelzer J Wilms R Staubert D Gruber R Rothschild Astron. Astrophys. 342 736 1999 1999A&A...342..736S Accretion Binaries, X-ray accretion, accretion disks stars: individual (Hercules X-1) stars: neutron X-rays: stars We report on a pre-eclipse dip of the X-ray binary pulsar Her X-1 observed by the Rossi X-ray Timing Explorer (RXTE) in 1996 July. The energy spectra in the 3-18keV range can be described by the sum of two power-laws, one of which is modified by photoelectric absorption and by Thomson scattering in cold material, plus an iron emission line at 6.7keV. We present the evolution of the spectral parameters with a temporal resolution of 16s and show that the varying flux and spectrum can be interpreted solely by a time varying column density. The data do not appear to require non-solar abundances in the absorbing material, although a slight over-abundance of the metals cannot be ruled out. We also find that the lightcurve is characterized by symmetric substructures which can be successfully modeled by Gaussian profiles. The recurrence time of these substructures is on a timescale of a few minutes.
Parameters of Gaussians fitted to the first half of the dip lightcurve Nsub Numeration of substructures observed in the lightcurve --- n_Nsub Note on Nsub number=1 Gaussians marked by an asterisk describe the underlying continuous intensity modulation and have been held fixed in the fit. --- Norm Normalization (depth of the Gaussian) ct/s Tcenter JD time of the line center d FWHM FWHM of Gaussian s table2.ps PostScript version of table2 table2.tex LaTeX version of table2 Patricia Bauer CDS 1998 Nov 30 Beate Stelzer <stelzer@xray.mpe.mpg.de> J_A+A_342_736.xml Dust extinction and intrinsic SEDs of carbon-rich stars. II. The hot carbon stars J/A+A/342/773 J/A+A/342/773 Hot carbon stars B-V colour excess Dust extinction and intrinsic SEDs of carbon-rich stars. II. The hot carbon stars J Bergeat A Knapik B Rutily Astron. Astrophys. 342 773 1999 1999A&A...342..773B III/156 : Cool Galactic Carbon Stars, 2nd Edition (Stephenson 1989) II/214 : Combined General Catalogue of Variable Stars (Kholopov+ 1998) II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) J/A+A/321/236 : Reddening and fluxes of carbon stars, Paper I. (Knapik+ 1997) J/A+A/344/263 : Miras B-V colour excess. Paper III. (Knapik+, 1999) Photometry Stars, carbon circumstellar matter dust, extinction stars: AGB and post-AGB stars: carbon A study of 140 hot carbon and related stars. Table 3 contains our hot carbon stars (HC)-classification (see section 2.2 in the paper) for 119 hot carbon stars and their colour excess E(B-V) as determined by the method described in section 2.3. The analogous data for 21 peculiar stars (RCB variables, AC Her [a RV Tau star], V553 Cen [a class II-Cepheid] etc...) can be found in Table 4: most of them have an oxygen-type classification.
HC-classification and colour excess for 119 hot carbon stars GCCS Stephenson's Catalogue (1989, Cat. <III/156>) number --- Name GCVS or NSV or HD or BD/CD or IRAS-PSC number number=1 General Catalogue of Variable Stars, Kholopov et al., 1985, or New Suspected Variables (NSV), see Cat. <II/214> or HD (cat. <III/135>) or BD (Cat. <I/122>) or CD-catalogues (Cat. <I/114>) or IRAS-PS Catalogue (Cat. <II/125>) --- GLON Galactic longitude deg GLAT Galactic latitude deg Class Hot Carbon star classification (0 to 5) --- E(B-V) Excess in the B-V colour index mag Oxygen-type or HC-classification and colour excess for 21 R CrB variables, hot carbon and related GCCS Stephenson's Catalogue (1989, Cat. <III/156>) number --- name GCVS or NSV or HD entry number=1 General Catalogue of Variable Stars, Kholopov et al., 1985, or New Suspected Variables (NSV), see Cat. <II/214> or HD (cat. <III/135>) IT Vir = HD 121447, NSV 3024 = HD 46407 and NSV 13571 = HD 201626 --- GLON Galactic longitude deg GLAT Galactic latitude deg Group Oxygen-type or Hot Carbon star classification --- E(B-V) Excess in the B-V colour index mag Jacques Bergeat CRAL Patricia Bauer CDS 1998 Nov 26 Jacques Bergeat <jb@cumulus.univ-lyon1.fr> J_A+A_342_773.xml Uncertainties in the solar system r-abundance distribution J/A+A/342/881 J/A+A/342/881 Uncertainties in r-abundance distribution Uncertainties in the solar system r-abundance distribution S Goriely Astron. Astrophys. 342 881 1999 1999A&A...342..881G Atomic physics nuclear reactions, nucleosynthesis, abundances solar system: general stars: abundances Sun: abundances Tables 1&2 correspond to the first estimate of the error factors affecting the {beta} decay rates of highly ionized heavy atoms in stellar environments. The uncertainties in the stellar {beta}-decay and EC rates strongly depend on the relevance of the experimentally unknown transitions at a given temperature and density and the reliability of their evaluated probability. To estimate the temperature- and density-dependent errors on the {beta}-decay rates, we have reiterated the Yokoi & Takahashi (1987, At. Data Nucl. Data Tables 36, 375) calculation with unknown transition rates modified by a typical error value of log(ft)=+/-0.5 (Takahashi 1998, private communication). No transition faster than log(ft)=5 is permitted in this error calculation. Newly measured transition probabilities, e.g. the allowed transition in the ^187^Re bound-state {beta}-decay (Bosch et al., 1996PhRvL..77.5190B), have been considered. Minimum and maximum error factors around the published rates of Yokoi & Takahashi (1987) are given in Tables 1 and 2 at temperatures 1<=T_8_<=4 and electronic densities (expressed in terms of 10^26^cm^-3^ of 1<=N_e_<=30. When the density-dependence does not affect the final uncertainty factor by more than 0.10 between the N_e_=1 and 3 cases, only values at N_e_=10 are given in the tables. Note that an increase of transition probability by log(ft)=0.5 gives rise to an increase of the final rate by a maximum value of 3.16. This maximum variation is obtained for many rates. The derived error factors are used in parametric s-process calculations within the canonical multi-event model to estimate their impact on the predicted s-abundance distribution and the resulting uncertainties on the solar r-abundance distribution.
Minimum and maximum error factors affecting the {beta}^-^ decay rates of Yokoi & Takahashi (1987, At. Data Nucl. Data Tables 36, 375) Minimum and maximum error factors affecting the {beta}^+^ and EC rates of Yokoi & Takahashi (1987, At. Data Nucl. Data Tables 36, 375) A Atomic mass of the nucleus --- Z Symbol the element --- Ne Electronic number density 10+26cm-3 T=1Min Minimum error factor for T=10+8K --- T=1Max Maximum error factor for T=10+8K --- T=2Min Minimum error factor for T=2*10+8K --- T=2Max Maximum error factor for T=2*10+8K --- T=3Min Minimum error factor for T=3*10+8K --- T=3Max Maximum error factor for T=3*10+8K --- T=4Min Minimum error factor for T=4*10+8K --- T=4Max Maximum error factor for T=4*10+8K --- tables.ps PostScript version of the tables tables.tex LaTeX version of the tables Patricia Bauer CDS 1998 Oct 26 Stephane Goriely <sgoriely@astro.ulb.ac.be> J_A+A_342_881.xml Late A-type stars: new Stroemgren photometric calibrations of absolute magnitudes from Hipparcos J/A+A/343/446 J/A+A/343/446 VRI Cousins photometry of Am stars Late A-type stars: new Stroemgren photometric calibrations of absolute magnitudes from Hipparcos A Domingo F Figueras Astron. Astrophys. 343 446 1999 1999A&A...343..446D I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Photometry, UBVRI Stars, early-type Hertzsprung-Russell (HR diagram) stars: chemically peculiar stars: distances stars: early-type stars: fundamental parameters Tablea1 contains photoelectric VRI Cousins photometry for 63 Am stars observed on the 17th June, 1996 with the 1.52m telescope of the Observatorio Astronomico Nacional (O.A.N.) at Calar Alto (Almeria, Spain), and on the 25th and 26th of the same month using the 1m Jakobus Kapteyn telescope at the Observatorio del Roque de los Muchachos (O.R.M., Canary Islands, Spain). The reduction procedure followed is explained in Rossello et al. (1985A&AS...59..399R) and Landolt (1983, Cat. <II/118>; 1983AJ.....88..853L) standard stars were used. We provide the V magnitude, the (V-R) and (V-I) colour indices, their associated standard errors and the number of observations performed for each star.
V, (V-R) and (V-I) of 63 Am stars HIP Hipparcos (Cat. <I/239>) number --- HD/BD HD (Cat. <III/135>) or BD (Cat. <I/122>) number --- Vmag V magnitude mag e_Vmag Standard error on V magnitude mag V-R (V-R) colour index mag e_V-R Standard error on V-R mag V-I (V-I) colour index mag e_V-I Standard error on V-I mag o_Vmag Number of observations --- Note 'D' if information about duplicity is available number=1 HIP 1286: Joint photometry, system identified as multiple in the Hipparcos Input Catalogue (Turon et al., 1992, Cat. <I/191>, hereafter HIC), CCDM 00161+0807 theta=142, rho=6.0, Delta m=4.5 HIP 2280: Joint photometry, system identified as multiple in HIC, CCDM 00291+1119 theta=304, rho=4.0, Delta m=6.2 HIP 63179: Joint photometry, system identified as multiple in HIC, CCDM 12566+4333 theta=211, rho=6.9, Delta m=5.5 HIP 64692: Joint photometry, system identified after publication of HIC, CCDM 13555+4051 theta=21, rho=0.37, Delta m=3.6 (from Hipparcos and Tycho Catalogues, ESA 1997, Cat. <I/239>; hereafter HIP) HIP 87641: Joint photometry, determined multiple by HIP, CCDM 17541+4702 theta=162, rho=0.30, Delta m=2.04 HIP 99159: Joint photometry, determined multiple by HIP, CCDM 20079+4600 theta=5, rho=2.91, Delta m=3.61 HIP 99211: Joint photometry, system identified as multiple in HIC, CCDM 20085+4622 theta=43, rho=4.17, Delta m=3.03 (from HIP) HIP 114501: Joint photometry, theta approx 180, rho approx 5, Delta m approx 5 theta: position angle relative to reference component, from North to the East (units are degrees) rho: separation between components (units are arcsec) Delta m: difference of magnitudes between components (units are mag) --- A. Domingo Universitat de Barcelona Patricia Bauer CDS 1999 Feb 23 Francesca Figueras, Albert Domingo <cesca@mizar.am.ub.es> J_A+A_343_446.xml A narrowband imaging survey of symbiotic stars J/A+A/343/841 J/A+A/343/841 Imaging of symbiotic stars A narrowband imaging survey of symbiotic stars R L M Corradi E Brandi O E Ferrer H E Schwarz Astron. Astrophys. 343 841 1999 1999A&A...343..841C III/174 : Atlas of line profiles of symbiotic stars (VanWinckel+, 1994) Spectrophotometry Stars, variable binaries: symbiotic ISM: jets and outflows surveys Narrowband images of 51 symbiotic stars were obtained at the ESO and ORM observatories to search for resolved optical nebulae. Ionized nebulae much larger than previously known are found around CH Cyg, HM Sge and V1016 Cyg, and they will be discussed in detail in forthcoming papers. A nebula with a deconvolved size between 0.9" and 1.5" is found around the symbiotic Mira H 1-36. The radio sources located few arcminutes aside of R Aqr (Hollis et al., 1987ApJ...321L..55H), which were suggested to be the remnant of a prehistoric eruption of the system, are found to be background galaxies. We also present a bibliographical compilation, updated to October 1998, of all the extended nebulae around symbiotic stars detected at optical and radio wavelengths, as well as a list of optical non-detections. The statistics of occurrence of these large ionized nebulae among symbiotic stars is discussed. Extended ionized nebulae appear to be a common component of the D-type symbiotics, and we infer that they are formed by the Mira wind and/or high velocity winds ejected by the hot component during outbursts. On the contrary, very few nebulae are detected around the systems containing normal red giants.
Optical non-detections Name1 First name of the object --- Name2 Second name (only when existing) --- IRType Symbiotic IR type --- Tel Telescope number=1 2.6NOT: 2.6m Nordic Optical Telescope of the ORM 1.5DAN: 1.54m Danish telescope of ESO 3.5NTT: 3.5m NTT of ESO 0.9DUT: 0.9m Dutch telescope of ESO 1SAAO : 1m telescope at the South African Astronomical Observatory --- Filter Filter number=2 Ha+[NII]: relatively broad filter (FWHM>=5nm) including both H{alpha} and [NII] emission Ha or [NII]: narrow filter isolating one of the two lines, with no or little contamination from the other (FWHM=2.5nm at the 1.5DAN, 1nm at the 2.6NOT) [OIII]: [OIII]500.7nm [OII]: [OII]372.8nm Ha cont.: off-band filter (continuum) --- ExpTime Exposure time number=3 (C) = coronographic spot s See Seeing arcsec Notes Notes number=4 saturated: indicated only when all exposures in a specific filter produced saturated images of the central source. 1: Munari & Patat, 1993A&A...277..195M 2: Kohoutek, 1997A&AS..125..445K 3: Extended nebula detected by Paresce (1990ApJ...357..231P), using a coronograph and after substraction of a stellar profile 4: A sub-arcsec nebula was detected by HST (Schild & Schmid, 1997A&A...324..606S) 5: An H{alpha} nebula with a size of 8 arcsec was detected by Fuensalida et al. (1988A&A...191L..13F) 6: No field stars available for comparison --- Patricia Bauer CDS 1999 Jan 05 Romano Corradi <rcorradi@ll.iac.es> J_A+A_343_841.xml On the local radio luminosity function of galaxies. I: the Virgo cluster J/A+A/343/86 J/A+A/343/86 Virgo cluster radio luminosity function. I. On the local radio luminosity function of galaxies. I: the Virgo cluster G Gavazzi A Boselli Astron. Astrophys. 343 86 1999 1999A&A...343...86G J/A+A/343/93 : Local radio luminosity function of galaxies. II (Gavazzi+ 1999) Clusters, galaxy Galaxies, radio Morphology galaxies: fundamental parameters galaxies: individual (Virgo cluster) galaxies: luminosity function, mass function radio continuum: galaxies We cross-correlate the galaxies brighter than m_B_=18 in the Virgo cluster with the radio sources in the NVSS survey (1.4GHz), resulting in 180 radio-optical identifications. We determine the radio luminosity function of the Virgo galaxies, separately for the early- and late-types. Late-type galaxies develop radio sources with a probability proportional to their optical luminosity. In fact their radio/optical (R_B_) distribution is gaussian, centered at log R_B_~-0.5, i.e. the radio luminosity is ~0.3 of the optical one. The probability of late-type galaxies to develop radio sources is almost independent of their detailed Hubble type, except for Sa (and S0+S0a) which are a factor of ~5 less frequent than later types at any R_B_. Giant elliptical galaxies feed "monster" radio sources with a probability strongly increasing with mass. However the frequency of fainter radio sources is progressively less sensitive on the system mass. The faintest giant E galaxies (M_B_=-17) have a probability of feeding low power radio sources similar to that of dwarf E galaxies as faint as M_B_=-13.
Parameters of the detected galaxies VCC VCC denomination (Binggeli et al., 1985AJ.....90.1681B) --- Pmag Corrected photographic magnitude mag MType Morphological classification (VCC) --- Agg Membership to the individual Virgo clouds --- RAh Optical right ascension (B1950) h RAm Optical right ascension (B1950) min RAs Optical right ascension (B1950) s DE- Optical declination sign --- DEd Optical declination (B1950) deg DEm Optical declination (B1950) arcmin DEs Optical declination (B1950) arcsec RArh Radio right ascension (B1950) h RArm Radio right ascension (B1950) min RArs Radio right ascension (B1950) s DEr- Radio declination sign --- DErd Radio declination (B1950) deg DErm Radio declination (B1950) arcmin DErs Radio declination (B1950) arcsec R-Ooff Radio-optical offset arcsec Class Identification class number=1 1: pointlike radio sources with R<=3 2: extended sources not meeting the 3{sigma} criterion 3: dubious identifications not meeting the 3{sigma} criterion (not used in the following analysis) 4: pointlike sources whose radio-optical offset is within the optical extent of the galaxy --- S1.4GHz 1.4 GHz total flux density mJy Maj Radio source major axis arcsec Min Radio source minor axis arcsec r_S1.4GHz Reference to the 1.4 GHz data number=2 References: 6: Hummel, 1980A&AS...41..151H 8: Condon, 1987ApJS...65..485C 10: Kotanyi, 1980A&AS...41..421K 15: Condon et al., 1990ApJS...73..359C 19: Condon et al., 1998AJ....115.1693C (NVSS) --- Patricia Bauer CDS 1998 Nov 06 Giuseppe Gavazzi <Giuseppe.Gavazzi@uni.mi.astro.it> J_A+A_343_86.xml A photometric study of the W UMa-type system RZ Tauri J/A+A/343/894 J/A+A/343/894 RZ Tau UBVR photometry A photometric study of the W UMa-type system RZ Tauri G Djurasevic M Zakirov S Erkapic Astron. Astrophys. 343 894 1999 1999A&A...343..894D Binaries, eclipsing Photometry, UBVRI binaries: eclipsing stars: activity stars: individual (RZ Tau) The present study deals with the problem of the orbital and physical parameters' estimation of the W UMa type eclipsing binary RZ Tauri, based on the interpretation of new photometric U B V R observations.
RZ Tau HD 285892 04 36 37.7 +18 45 18
UBVR data for RZ Tau JD Hel Heliocentric Julian date d Phase Orbital phase --- Umag U magnitude mag Bmag B magnitude mag Vmag V magnitude mag Rmag R magnitude mag Patricia Bauer CDS 1998 Dec 08 Gojko Djurasevic <gdjurasevic@aob.bg.ac.yu> J_A+A_343_894.xml On the local radio luminosity function of galaxies. II: Environmental dependences among late-type galaxies J/A+A/343/93 J/A+A/343/93 Local radio luminosity function of galaxies. II. On the local radio luminosity function of galaxies. II: Environmental dependences among late-type galaxies G Gavazzi A Boselli Astron. Astrophys. 343 93 1999 1999A&A...343...93G VII/4A : Abell and Zwicky Clusters of Galaxies (Abell+ 1974) VII/190 : Zwicky Galaxy Catalog (Zwicky+ 1968) VIII/48 : The FIRST Survey (White+ 1997) J/A+A/343/86 : Local radio luminosity function of galaxies. I. (Gavazzi+ 1999) Clusters, galaxy Galaxies, radio Morphology galaxies: clusters: general galaxies: fundamental parameters galaxies: interactions galaxies: luminosity function, mass function intergalactic medium radio continuum: galaxies Using new extensive radio continuum surveys at 1.4GHz (FIRST and NVSS), we derive the distribution of the radio/optical and radio/NIR luminosity (RLF) of late-type (Sa-Irr) galaxies (m_p_<15.7) in 5 nearby clusters of galaxies: A262, Cancer, A1367, Coma and Virgo. With the aim of discussing possible environmental dependences of the radio properties, we compare these results with those obtained for relatively isolated objects in the Coma supercluster. We find that the RLF of Cancer, A262 and Virgo are consistent with that of isolated galaxies. Conversely we confirm earlier claims that galaxies in A1367 and Coma have their radio emissivity enhanced by a factor ~5 with respect to isolated objects. We discuss this result in the framework of the dynamical pressure suffered by galaxies in motion through the intra-cluster gas (ram-pressure). We find that the radio excess is statistically larger for galaxies in fast transit motion. This is coherent with the idea that enhanced radio continuum activity is associated with magnetic field compression. The X-ray luminosities and temperatures of Coma and A1367 imply that these two clusters have significantly larger intracluster gas density than the remaining three studied ones, providing a clue for explaining the higher radio continuum luminosities of their galaxies. Multiple systems in the Coma supercluster bridge (with projected separations smaller than 300kpc) have radio luminosities significantly larger than isolated galaxies.
Parameters of the detected galaxies Cluster Cluster name --- CGCG CGCG denomination (Z FFF-NNN in Simbad) (Zwicky et al., 1961-68, Cat. <VII/190>) --- m_CGCG Multiplicity index on CGCG --- Pmag Corrected photographic magnitude mag Hmag Corrected H band magnitude mag MType Morphological classification (VCC) --- Agg Membership to the individual clusters --- RAh Optical right ascension (B1950) h RAm Optical right ascension (B1950) min RAs Optical right ascension (B1950) s DE- Optical declination sign --- DEd Optical declination (B1950) deg DEm Optical declination (B1950) arcmin DEs Optical declination (B1950) arcsec RArh Radio right ascension (B1950) h RArm Radio right ascension (B1950) min RArs Radio right ascension (B1950) s DEr- Radio declination sign --- DErd Radio declination (B1950) deg DErm Radio declination (B1950) arcmin DErs Radio declination (B1950) arcsec R-Ooff radio-optical offset (arcsec) arcsec Class Identification class number=1 1: pointlike radio sources with R<=3 2: extended sources not meeting the 3{sigma} criterion 3: dubious identifications not meeting the 3{sigma} criterion (not used in the following analysis) 4: pointlike sources whose radio-optical offset is within the optical extent of the galaxy --- S1.4GHz 1.4 GHz total flux density (mJy) mJy Maj Radio source major axis (arcsec) arcsec Min Radio source minor axis (arcsec) arcsec r_S1.4GHz Reference to the 1.4 GHz data number=2 References: 1: Jaffe & Gavazzi, 1986AJ.....91..204J 5: del Castillo et al., 1988AJ.....95.1340D 6: Hummel, 1980A&AS...41..151H 7: Gioia & Fabbiano, 1987ApJS...63..771G 8: Condon, 1987ApJS...65..485C 13: Salpeter & Dickey, 1987, Cat. <J/ApJ/317/102> 16: Gavazzi & Contursi, 1994AJ....108...24G 17: White et al., 1997, Cat. <VIII/51> (FIRST) 18: Bravo-Alfaro, 1997, Ph.D. Thesis, University of Paris 19: Condon et al., 1998AJ....115.1693C (NVSS) --- Patricia Bauer CDS 1998 Nov 06 Giuseppe Gavazzi <Giuseppe.Gavazzi@uni.mi.astro.it> J_A+A_343_93.xml Dust extinction and intrinsic SEDs of carbon-rich stars. III. The Miras, CS and SC stars J/A+A/344/263 J/A+A/344/263 B-V colour excess of Miras Dust extinction and intrinsic SEDs of carbon-rich stars. III. The Miras, CS and SC stars A Knapik J Bergeat B Rutily Astron. Astrophys. 344 263 1999 1999A&A...344..263K III/156 : Cool Galactic Carbon Stars, 2nd Edition (Stephenson 1989) II/214 : Combined General Catalogue of Variable Stars (Kholopov+ 1998) J/A+A/321/236 : Reddening and fluxes of carbon stars, Paper I. (Knapik+ 1997) J/A+A/342/773 : Hot carbon stars B-V colour excess, Paper II. (Bergeat+ 1999) Photometry Stars, carbon Stars, variable circumstellar matter dust, extinction stars: AGB and post-AGB stars: carbon A study of 73 carbon-rich Miras (see Subsec. 6.1) with suitable solution for 56 stars at one or several phase of their variations. In the second part, preliminary and incomplete results are reported for 17 additional Miras observed at only one phase. Table 5 contains our HC-CV-classification (see text) for the stars and their colour excess E(B-V) as determined by the method described in Subsec. 2.2.
HC-CV-SCV classification and colour excess E(B-V) CGCS Stephenson's Catalogue (Cat. <III/156>) entry --- Note Note number=1 The table contains two parts: 56 Miras in the first one are satisfactionally studied at one or several phases, while preliminary and incomplete data are given in the second part for 17 additional Miras at a single phase (with an *). --- GCVS GCVS (Cat. <II/214>) entry --- GLON Galactic longitude deg GLAT Galactic latitude deg Phase Phase of variations --- u_Phase Uncertainty flag on Phase --- n_Phase Note on Phase number=2 i: intermediary phase, M: maximum light , m: minimum light, ?: unknown --- Class HC5 or CV (1 to 7) or SCV classification --- E(B-V) Excess in the B-V colour index mag u_E(B-V) Uncertainty flag on E(B-V) --- l_E'(B-V) Limit flag on E'(B-V) --- E'(B-V) Field colour excess from the literature mag u_E'(B-V) Uncertainty flag on E'(B-V) --- IRFilter Filter of first occurrence of the IR excess number=3 Name of the IR filter where some excess due to thermal emission from dust is first observed (no is quoted when no excess is found up to IRAS [25]). --- Remarks Remarks and/or additional information --- Jacques Bergeat CRAL Patricia Bauer CDS 1999 Jan 15 Jacques Bergeat <jb@cumulus.univ-lyon1.fr> J_A+A_344_263.xml Sh 138: a compact HII region excited by a very young cluster J/A+A/344/943 J/A+A/344/943 Sh 138 BVRIJHK photometry Sh 138: a compact HII region excited by a very young cluster L Deharveng A Zavagno D Nadeau J Caplan M Petit Astron. Astrophys. 344 943 1999 1999A&A...344..943D Clusters, open H II regions Photometry, UBVRIJKLMNH HII regions infrared: stars ISM: individual (Sh 138) open clusters and associations: individual (Sh 138) stars: pre-main sequence We present a photometric and spectroscopic study of the compact HII region Sh 138 and its associated stellar cluster. The positions and BVRIJHK magnitudes are obtained for more than 400 stars over a field of about 4' square centred on the HII region. Sh 138 is excited by a cluster of young massive stars. At the cluster's very centre are at least four O-B2 stars separated by less than 4". The brightest of these, both in the visible and the near infrared, exhibits a spectrum similar to those of the more massive Herbig Ae/Be stars. This star, our No. 183, is overluminous by a factor of 2.5 in the visible and four in the near IR with respect to the O9.5V star required to account for the ionization level of the HII region. However star 183's position in the J-H versus H-K diagram does not indicate a near-IR excess. We suggest that this star is a young massive object belonging to a binary or multiple system. The stellar cluster associated with Sh 138 is very reminiscent of the Orion Trapezium cluster: it is centrally peaked around several massive stars, and is dense - more than 550stars/pc^2^ at its centre. The visual extinction in the cluster varies between 5mag and more than 35mag; large variations are observed over very small scales (for example, more than 20mag over less than 4" among the central massive stars).
Coordinates and photometry of all the stars Seq Running number of the star --- Xpos tangential coordinate number=1 Xpos and Ypos are with respect to RA=22h32m45.6s, Dec=58{deg}28'16.8" arcmin Ypos tangential coordinate number=1 Xpos and Ypos are with respect to RA=22h32m45.6s, Dec=58{deg}28'16.8" arcmin RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Vmag V magnitude mag B-V B-V colour index mag V-R V-R colour index mag R-I R-I colour index mag V-I V-I colour index mag Kmag K magnitude mag J-K J-K colour index mag J-H J-H colour index mag H-K H-K colour index mag Patricia Bauer CDS 1999 Feb 01 James Caplan <caplan@observatoire.cnrs-mrs.fr> J_A+A_344_943.xml Star formation history of early-type galaxies in low density environments. V. Blue line-strength indices for the nuclear region J/A+A/345/419 J/A+A/345/419 Star formation in early-type galaxies Star formation history of early-type galaxies in low density environments. V. Blue line-strength indices for the nuclear region M Longhetti A Bressan C Chiosi R Rampazzo Astron. Astrophys. 345 419 1999 1999A&A...345..419L J/A+AS/130/251 : Star Formation in Early-type galaxies. I. (Longhetti+ 1998) J/A+A/311/361 : Evolution models of elliptical galaxies. II. (Tantalo+, 1996) III/92 : A Library of Stellar Spectra (Jacoby+ 1984) Longhetti et al., Paper I. 1998A&AS..130..251L, Cat. <J/A+AS/130/251> Longhetti et al., Paper II. 1998A&AS..130..267L Rampazzo et al., Paper III. 1999A&A...341..357R Galaxies, spectra Models, evolutionary galaxies: elliptical and lenticular, cD galaxies: evolution galaxies: formation galaxies: fundamental parameters galaxies: interactions galaxies: starburst We analyze the star formation properties of a sample of 21 shell galaxies and 30 early-type galaxies members of interacting pairs, located in low density environments (Longhetti et al., 1998, Cat. <J/A+AS/130/251>, 1998A&AS..130..267L). The study is based on new models developed to interpret the information coming from `blue' H{delta}FeI, H+K(CaII) and D4000 line-strength indices proposed by Rose (1984AJ.....89.1238R; 1985AJ.....90.1927R) and Hamilton (1985ApJ...297..371H). We find that the last star forming event that occurred in the nuclear region of shell galaxies is statistically old (from 0.1 up to several Gyr) with respect to the corresponding one in the sub-sample of pair galaxies (<0.1Gyr or even ongoing star formation). If the stellar activity is somehow related to the formation of shells, as predicted by several dynamical models of galaxy interaction, shells have to be considered long lasting structures. Since pair members show evidence of very recent star formation, we suggest that either large reservoirs of gas have to be present to maintain active star formation, if these galaxies are on periodic orbits, or most of the pair members in the present sample are experiencing unbound encounters.
Blue indices for Simple Stellar Populations (SSP) Log(age) Logarithm of age [yr] D4000a Index {Delta}4000 at Z=0.004 --- H+K(CaII)a Index H+K(CaII) at Z=0.004 --- Hd/FeIa Index H{delta}/FeI at Z=0.004 --- D4000b Index {Delta}4000 at Z=0.02 --- H+K(CaII)b Index H+K(CaII) at Z=0.02 --- Hd/FeIb Index H{delta}/FeI at Z=0.02 --- D4000c Index {Delta}4000 at Z=0.05 --- H+K(CaII)c Index H+K(CaII) at Z=0.05 --- Hd/FeIc Index H{delta}/FeI at Z=0.05 --- Patricia Bauer CDS 1999 Apr 26 Marcella Longhetti <longhett@iap.fr> J_A+A_345_419.xml B-type pulsators in the central region of NGC 869 (h Persei) J/A+A/345/505 J/A+A/345/505 UBVI magnitudes of NGC 869 B-type pulsators B-type pulsators in the central region of NGC 869 (h Persei) J Krzesinski A Pigulski Z Kolaczkowski Astron. Astrophys. 345 505 1999 1999A&A...345..505K J/A+A/325/987 : UBV magnitude of NGC 884 B-type pulsators (Krzesinski+ 1997) Binaries, eclipsing Photometry, UBVRI Stars, B-type binaries: eclipsing open clusters and associations: individual (NGC 869, h Per) stars: oscillations stars: variables: general In the course of the search for B-type pulsators in the central region of h Persei, we discovered two {beta} Cephei stars, Oo692 and Oo992, and one SPB star, Oo893. The first two stars are monoperiodic pulsators with periods of 0.1716946 and 0.1326359 d respectively, and semi-amplitudes smaller than 0.01mag. The light curve of Oo893 can be described by a single 1.193633-day period, slightly non-sinusoidal in shape, and having semi-amplitudes from 19 mmag in I to 48 mmag in U. Oo893 is the first SPB star found in h and {chi} Persei. In addition, we discovered seven other variables, including three eclipsing binaries and one {lambda} Eri star. One of the binaries is a W UMa-type star and a likely cluster member. We also present new UBV photometry for 258 stars in the field. The average reddening, estimated from the cluster colour-colour diagram, amounts to E(B-V)=0.52mag. A 0.1mag dispersion of reddenings within the cluster is also seen.
UBV photometry of stars in h Persei Xpos X position number=1 1pix~0.15', see figure 1. pix Ypos Y position number=1 1pix~0.15', see figure 1. pix OO Oosterhoff (1937AnLei..17a...1O) number (Cl* NGC 6171 Oos NN in Simbad) --- W Wildey (1964ApJS....8..439W) number (Cl* NGC 869 W NNNa in Simbad) --- m_W Multiplicity index or uncertainty flag on W --- MV Moffat & Vogt (1974VeBoc...2....1M) number (Cl* NGC 6171 MV NNNNN in Simbad) --- m_MV Multiplicity index or uncertainty flag on MV --- Vmag V magnitude mag B-V B-V colour index mag r_B-V Reference to BV photometry number=2 S: star was observed from Suhora only B: star was observed from Bialkow only S+B: star was observed form Suhora and Bialkow --- n_B-V I: BV photometry transformed with the use of I-filter measurements --- U-B U-B colour index mag RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign (2000.0) --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec Rem Remarks --- VarFile Name of the File containing light curves in subdirectory curves --- </tableLink> </tableLinks> <fields> <field> <name>Filter</name> <definition>Filter</definition> <units>---</units> </field> <field> <name>HJD</name> <definition>Heliocentric Julian date</definition> <units>d</units> </field> <field> <name>Dmag</name> <definition>Differential magnitude in Filter band</definition> <units>mag</units> </field> </fields> </tableHead> <history> <ingest> <creator> <lastName>Patricia Bauer</lastName> <affiliation>CDS</affiliation> </creator> <date> <year>1999</year> <month>Apr</month> <day>22</day> </date> <acknowledgement>Andrzej Pigulski <pigulski@astro.uni.wroc.pl></acknowledgement> </ingest> </history> <identifier>J_A+A_345_505.xml</identifier> </dataset> <dataset subject="astronomy" xmlns:xlink="http://www.w3.org/XML/XLink/0.9"> <title>BVRI photometry of the star-forming region NGC 2264: the initial mass function and star-forming rate J/A+A/345/521 J/A+A/345/521 BVRI photometry of NGC 2264 BVRI photometry of the star-forming region NGC 2264: the initial mass function and star-forming rate E Flaccomio G Micela S Sciortino F Favata C Corbally A Tomaney Astron. Astrophys. 345 521 1999 1999A&A...345..521F Clusters, open Photometry, UBVRI Stars, pre-main sequence open clusters and associations: individual (NGC 2264) stars: formation stars: late-type stars: pre-main sequence The pre-main-sequence (PMS) population in the mass range between =~0.2 and =~3M_{sun}_ in southern part of the star-forming region NGC 2264 has been studied, determining both the Initial Mass Function in the region as well as the star-formation rates for different mass ranges. The sample is a composite one, derived through the union of samples obtained through different techniques and each suffering from different biases: previously known PMS stars in the region from the literature, photometrically-selected T Tauri candidates (from our own photometric data, discussed in detail in the present paper) and X-ray selected PMS candidates (discussed in detail in a companion paper) have been joined to form a sample which we show to be statistically complete (i.e. free from the biases which affect each of the parent samples) down to =~0.6M_{sun}_ (while being incomplete at lower masses). Individual masses and ages have been derived by placing the individual stars on evolutionary tracks, allowing us to derive both the IMF and the star formation rate. The Initial Mass Function thus derived for NGC 2264 shows evidence for a bimodal distribution of masses, with a break in the IMF at around 1M_{sun}_.
Catalog of CCD photometry Seq Sequential number --- n_Seq + when present in table5.dat file --- uPhot 1: Uncertain photometry --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag Visual magnitude mag B-V B-V colour index mag V-R V-R colour index mag R-I R-I colour index mag Catalog of observed NGC 2264 members Seq Identification number --- uPhot 1: uncertain photometry --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag Visual Magnitude mag B-V B-V colour Index mag V-R V-R colour Index mag R-I R-I colour Index mag Log(Lbol) Bolometric Luminosity [solLum] Log(Teff) Effective Temperature [K] Mass Mass solMass Log(Age) Logarithm of Age [yr] Memb Membership criteria number=1 Membership criteria: c: this paper (see text); x: Flaccomio et al. (in prep.); h: Herbig (1954ApJ...119..483H), Marcy (1980AJ.....85..230M), Ogura (1984PASJ...36..139O) or Sung et al. (1997AJ....114.2644S) p: Vasilevskis et al. (1965AJ.....70..797V) with membership probabilities >50%. --- Ident Cross identifications number=2 A prefix, indicating the original catalog, is followed by the reference number used by the authors of the catalog. The prefixes stand for: W: Walker (1956ApJS....2..365W) V: Vasilevskis et al. (1965AJ.....70..797V) S: Sung et al. (1997AJ....114.2644S) O: Ogura (1984PASJ...36..139O) M: Marcy (1980AJ.....85..230M) H: Herbig (1954ApJ...119..483H) FX: Flaccomio et al. (in prep.) --- Patricia Bauer CDS 1999 Apr 27 Ettore Flaccomio <ettoref@oapa23.astropa.unipa.it> J_A+A_345_521.xml Abundance gradients in the outer galactic disk form planetary nebulae J/A+A/345/629 J/A+A/345/629 Abundance gradients in planetary nebulae Abundance gradients in the outer galactic disk form planetary nebulae W J Maciel C Quireza Astron. Astrophys. 345 629 1999 1999A&A...345..629M V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+ 1992) J/A+A/282/436 : Abundance gradients from disk PNs (Maciel+ 1994) J/A+A/313/924 : Relative fluxes in 11 type I PN (Costa+, 1996) Abundances, peculiar Planetary nebulae Galaxy: abundances ISM: abundances planetary nebulae: general Radial abundance gradients of the element ratios O/H, Ne/H, S/H, and Ar/H are determined on the basis of a sample of disk planetary nebulae. The behaviour of the gradients at large distances from the galactic centre, R>R_0_=7.6kpc, is emphasized. It is concluded that the derived gradients are consistent with an approximately constant slope in the inner parts of the Galaxy, and some flattening for distances larger than R_0_. A comparison is made with previous determinations using both photoionized nebulae and young stars, and some consequences on theoretical models for the chemical evolution of the galactic disk are discussed.
Data for disk planetary nebulae Name Common name of the nebula --- PNG PNG catalogue number --- Dist Distance kpc GDist Galactocentric distance kpc O/H O/H abundance in the form: log (O/H) + 12 --- Ne/H Ne/H abundance in the form: log (Ne/H) + 12 --- S/H S/H abundance in the form: log (S/H) + 12 --- Ar/H Ar/H abundance in the form: log (Ar/H) + 12 --- Ref Reference of the abundances number=1 1 - Maciel and Koeppen (1994, Cat. <J/A+A/282/436>) 2 - Costa et al. (1996A&AS..116..249C) 3 - Costa et al. (1997, in: Advances in stellar evolution, Rood, R.T., Renzini, A. (eds.), CUP, Cambridge, 159) 4 - Corradi et al. (1997A&A...322..975C) 5 - Hajian et al. (1997ApJ...487..304H) 6 - Kingsburgh and Barlow (1994MNRAS.271..257K) 7 - Perinotto et al. (1994A&AS..107..481P) 8 - Perinotto (1991ApJS...76..687P) 9 - Koeppen et al. (1991A&A...248..197K) --- table1.tex TeX version of table1 Patricia Bauer CDS 1999 Mar 04 Walter J. Maciel <maciel@orion.iagusp.usp.br> J_A+A_345_629.xml Photometric parameters for rotating models of A- and F-type stars J/A+A/346/586 J/A+A/346/586 Rotating models of A and F stars Photometric parameters for rotating models of A- and F-type stars F Perez Hernandez A Claret M M Hernandez E Michel Astron. Astrophys. 346 586 1999 1999A&A...346..586P Models, atmosphere Photometry, Geneva Photometry, UBV Photometry, uvby Stars, A-type Stars, F-type delta Scuti open clusters and associations: individual (Praesepe) stars: fundamental parameters stars: rotation Magnitude differences between rotating and non-rotating copartners for a grid of models with solar metallicity are tabulated here. The results are expressed in terms of the dimensionless angular velocity w-bar- defined in Eq.(1) of the paper, the angle of inclination i and the atmospheric parameters T_e_ and g_e_ defined in Eqs.(22) and (21), respectively. To obtain the absolute magnitudes for a given rotating model, the magnitudes of a non-rotating model with T_eff_=T_e_, g=g_e_ and the same intrinsic luminosity must be added. Results are given for the filters in the Geneva, Johnson and Stroemgren systems. Eq (1): w-bar = {Omega}/{Omega}_c_, where {Omega} is the angular velocity of the star, and {Omega}_c_^2^=8GM/(27R^3^_p_), where M is the mass and R_p_ the polar radius.
Geneva photometry logTe Electron temperature atmospheric parameter number=1 Te {prop.to} L/(4{pi}{sigma}R^2^_p_) = Eq (22). [K] logge Electron surface gravity atmospheric parameter [cm/s2] w-bar Dimensionless angular velocity --- i Angle of inclination deg DBmag Magnitude difference in filter B mag DUmag Magnitude difference in filter U mag DVmag Magnitude difference in filter V mag DB1mag Magnitude difference in filter B1 mag DB2mag Magnitude difference in filter B2 mag DV1mag Magnitude difference in filter V1 mag DGmag Magnitude difference in filter G mag Johnson and Stroemgren photometry logTe Electron temperature atmospheric parameter number=1 Te{prop.to}L/(4{pi}{sigma}R^2^_p_) = Eq (22). [K] logge Electron surface gravity atmospheric parameter [cm/s2] w-bar Dimensionless angular velocity --- i Angle of inclination deg DUmag Magnitude difference in filter U mag DBmag Magnitude difference in filter B mag DVmag Magnitude difference in filter V mag Dumag Magnitude difference in filter u mag Dvmag Magnitude difference in filter v mag Dbmag Magnitude difference in filter b mag Dymag Magnitude difference in filter y mag Patricia Bauer CDS 1999 Apr 22 Fernando Perez <fph@ll.iac.es> J_A+A_346_586.xml Mapping the contours of the Local Bubble: Preliminary results J/A+A/346/785 J/A+A/346/785 NaI in Local Bubble Mapping the contours of the Local Bubble: Preliminary results D Sfeir R Lallement F Crifo B Y Welsh Astron. Astrophys. 346 785 1999 1999A&A...346..785S Abundances Interstellar medium ISM: bubbles ISM: structure solar neighborhood We present preliminary results form a long-term program of mapping the neutral absorption characteristics of the local interstellar medium, taking advantage of Hipparcos stellar distances. Equivalent width of the NaI D-line doublet at 5890{AA} are presented for the lines-of-sight towards some 143 new target stars lying within 300pc of the Sun.
List of stars observed at OHP HD HD number --- n_HD *: Redundant observations with Paper 1 (Welsh et al., 1998A&A...333..101W) --- GLON Galactic longitude deg GLAT Galactic latitude deg Dist Hipparcos distance pc SpType Spectral type --- Vmag Visual magnitude mag l_EWD2 Uncertainty flag on EWD2 --- EWD2 Equivalent width of the sodium doublet D2 line 5889.9512{AA} 0.1pm u_EWD2 Uncertainty flag on EWD2 --- l_EWD1 Uncertainty flag on EWD1 --- EWD1 Equivalent width of the sodium doublet D1 line 5895.9243{AA} 0.1pm u_EWD1 Uncertainty flag on EWD1 --- Other published NaI observations used in the paper HD HD number --- Name Star name --- GLON Galactic longitude deg GLAT Galactic latitude deg Dist Hipparcos distance pc l_EWD2 Limit flag on EWD2 --- EWD2 Equivalent width of the sodium doublet D2 line 5889.9512{AA} density 0.1pm l_EWD1 Limit flag on EWD1 --- EWD1 Equivalent width of the sodium doublet D1 line 5895.9243{AA} density (if avail.) 0.1pm l_logNaI Limit flag on logNaI --- logNaI Logarithm of the NaI column density (if avail.) cm-2 Ref Reference number number=1 1: Welsh et al. (1997ApJS..112..507W) 2: Benjamin et al. (1996ApJ...464..831B) 3: Sahu et al. (1998ApJ...504..522S) 4: Meyer et al. (1996ApJ...464L.179M) 5: Genova et al. (1997ApJ...484..761G) 6: Welty et al. (1994ApJ...436..152W) 7: Lyons et al. (1994A&A...286..535L) 8: Penprase et al. (1998ApJ...492..617P) 9: Grant and Burrows (1999, ApJ, submitted) --- Note Notes number=2 a: W_{lambda}_(D2) derived from N_(NaI)__TOT_ b: W_{lambda}_(D2) derived from W_{lambda}_(D1) c: Redundant observations with Paper 1 (Welsh et al., 1998A&A...333..101W) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1999 May 06 Rosine Lallement <Rosine.Lallement@aerov.jussieu.fr> J_A+A_346_785.xml Interstellar dust and magnetic field at the boundaries of the Local Bubble Analysis of polarimetric data in the light of Hipparcos parallaxes J/A+A/346/955 J/A+A/346/955 Magnetic field around the Local Bubble Interstellar dust and magnetic field at the boundaries of the Local Bubble Analysis of polarimetric data in the light of Hipparcos parallaxes J L Leroy Astron. Astrophys. 346 955 1999 1999A&A...346..955L I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Polarization ISM: clouds ISM: magnetic fields polarization solar neighborhood This catalogue gathers optical polarimetric data, concerning 918 stars, observed by 15 different authors.
*Unpolarized stars: 60 pc < D < 90 pc Unpolarized stars: 90 pc < D < 120 pc Unpolarized stars: 120 pc < D < 150 pc Unpolarized stars: D > 150 pc Polarized stars: 60 pc < D < 90 pc Polarized stars: 90 pc < D < 120 pc Polarized stars: 120 pc < D < 150 pc HD HD number --- GLON Galactic longitude deg GLAT Galactic latitude deg D Distance to the Sun pc Pdeg Polarization degree 10-5 e_Pdeg rms uncertainty on P 10-5 PA Polarization angle in the Galactic system deg Ref Source of the polarimetric data number=1 1 : Appenzelller 1966ZA.....64..269 ; 1968ApJ...151..907A 2 : Behr 1959, Verroff. Univ. Sternw. Gottingen No 126 3 : Berdyugin et al. 1995A&A...294..568B 4 : Dyck and Jennings 1971AJ.....76..431D 5 : Klare et al. 1971A&A....11..155K 6 : Korhonen and Reiz 1986A&AS...64..487K 7 : Krautter 1980A&AS...39..167K 8 : Leroy 1993A&A...274..203 ; 1993, Cat. <J/A+AS/101/551> ; 1995, Cat. <J/A+AS/114/79> ; this work. 9 : Mathewson and Ford 1970MmRAS..74..139M 10 : Piirola 1977A&AS...30..213P 11 : Poeckert et al. 1979AJ.....84..812P 12 : Reiz and Franco 1998, Cat. <J/A+AS/130/133> 13 : Schr=94der 1976A&AS...23..125S 14 : Serkowski 1970ApJ...160.1083S ; 1975ApJ...196..261S 15 : Tinbergen 1981A&A...102...53V --- Patricia Bauer CDS 1999 Apr 22 Jean-Louis Leroy <leroy@obs-mip.fr> J_A+A_346_955.xml The Ap spectroscopic binary HD 59435 revisited J/A+A/347/164 J/A+A/347/164 HD 59435 Geneva photometry The Ap spectroscopic binary HD 59435 revisited G Wade G Mathys P North Astron. Astrophys. 347 164 1999 1999A&A...347..164W J/A+A/314/491 : HD 59435 radial velocity + Geneva photometry (Wade+ 1996) Photometry, Geneva Stars, Ap binaries: spectroscopic stars: chemically peculiar stars: evolution stars: individual (HD 59435) stars: magnetic fields The SB2 binary HD 59435 hosts a yellow giant and a magnetic Ap star, the latter being the secondary (Wade et al., 1996, Cat. <J/A+A/314/491>) and exhibiting spectral lines resolved into their magnetically-split components. Additional measurements of the magnetic field modulus of the Ap secondary are reported, as well as additional radial velocities for both components and photometric magnitudes and colours in the Geneva system. The magnetic field modulus varies with a period of about 1360 days. For a general description of the Geneva photometric system, see e.g. <GCPD/13>
HD 59435 07 29 35.41 -09 15 33.8
Visual magnitudes and colour indices of HD 59435 in the Geneva photometric system HJD Heliocentric Julian day d Q Photometric Q weight (Rufener, 1988, Cat. <II/169>) --- Vmag Magnitude in the visible mag P Photometric P weight (Rufener, 1988, Cat. <II/169>) --- [U-B] Geneva [U-B] index mag [V-B] Geneva [V-B] index mag [B1-B] Geneva [B1-B] index mag [B2-B] Geneva [B2-B] index mag [V1-B] Geneva [V1-B] index mag [G-B] Geneva [G-B] index mag Patricia Bauer CDS 1999 Apr 20 Pierre North <Pierre.North@obs.unige.ch> J_A+A_347_164.xml The solar abundance of iron and the photospheric model J/A+A/347/348 J/A+A/347/348 Solar abundance of iron The solar abundance of iron and the photospheric model N Grevesse A J Sauval Astron. Astrophys. 347 348 1999 1999A&A...347..348G J/A+A/274/555 : Asymmetry of FeI lines in solar spectrum (Stathopoulou+ 1993) J/A+A/340/300 : Fe II oscillator strengths (Raassen+ 1998) J/A+AS/102/269 : Lab. and solar highly-excited levels of Fe I (Nave+ 1993) Atomic physics Sun atomic data Sun: abundances Sun: photosphere Numerous papers on the solar photospheric abundance of iron have recently been published leading to a longstanding debate concerning rather different results obtained from the analyses of Fe I lines and, to a lesser extent, of Fe II lines. Based on a set of 65 solar Fe I lines, with accurate transition probabilities as well as new accurate damping constants, we construct a new empirical photospheric model. We succeed to reconcile abundance results obtained from low and high excitation Fe I lines as well as from Fe II lines and derive a solar photospheric abundance of iron, A_Fe_=7.50+/-0.05, which perfectly agrees with the meteoritic value.
New photospheric model logTau0 Logarithmic value of the optical depth at 500nm --- T Temperature K logPe Logarithmic value of the electron pressure (in dyne/cm2) 0.1Pa logPg Logarithmic value of the gas pressure (in dyne/cm2) 0.1Pa Patricia Bauer CDS 1999 Jun 17 Joan Vandekerckhove <Joan.Vandekerckhove@ksb-orb.oma.be> J_A+A_347_348.xml Long-term coherent variations in the WR system EZ CMa : The binary scenario revisited J/A+A/347/583 J/A+A/347/583 EZ CMa spectroscopy Long-term coherent variations in the WR system EZ CMa : The binary scenario revisited L N Georgiev G Koenigsberger M M Ivanov N St-Louis O Cardona Astron. Astrophys. 347 583 1999 1999A&A...347..583G J/A+AS/119/37 : EZ CMa UBV + VBLUW photometry (Duijsens+, 1996) Binaries, spectroscopic Spectroscopy binaries: spectroscopic stars: individual (HD 50896, EZ Cma, WR6) stars: variables: general stars: Wolf-Rayet The table contains the window averaged flux (WAF) in two windows located at the P Cyg absorption component of the NV 4604/4620 doublet and the kurtosis of the HeII 4540 and HeII 4686 lines of the star EZ CMa. The three data sets are stored in three different files with the same format.
EZ CMa HD 50896 WR 6 06 54 13.0 -23 55 42
WAF and Kurtosis for the SIT data WAF and Kurtosis for the SPM data WAF and Kurtosis for the Rozhen data JD Julian Date d WAV4604 Window averaged flux for the 4604{AA} window number=1 The units are arbitrary, because the spectra are normalized to the continuum. --- WAV4620 Window averaged flux for the 4620{AA} window number=1 The units are arbitrary, because the spectra are normalized to the continuum. --- KUR4686 Kurtosis for HeII 4686A line number=1 The units are arbitrary, because the spectra are normalized to the continuum. --- KUR4540 Kurtosis for HeII 4540A line number=1 The units are arbitrary, because the spectra are normalized to the continuum. --- Patricia Bauer CDS 1999 Jun 17 Leonid Georgiev <georgiev@astroscu.unam.mx> J_A+A_347_583.xml Early-type stars in the Galactic halo from the Palomar-Green Survey. II: A sample of distant, apparently young Population I stars J/A+A/347/69 J/A+A/347/69 Abundances of halo early-type stars Early-type stars in the Galactic halo from the Palomar-Green Survey. II: A sample of distant, apparently young Population I stars W R J Rolleston N C Hambly F P Keenan P L Dufton R A Saffer Astron. Astrophys. 347 69 1999 1999A&A...347...69R Abundances Equivalent widths Stars, early-type stars: abundances stars: atmospheres stars: early-type stars: kinematics We present echelle (R~40,000) spectroscopic observations for a sample of apparently normal, high Galactic latitude, early-type stars drawn from the Palomar-Green Survey. The metal-line spectra show evidence for rotational velocity broadening with values of vsini<=300km/s. In conjunction with Kurucz model atmospheres, we derive stellar photospheric abundances that are consistent with a Population I chemical composition; differential abundances with respect to Galactic disk Population I stars indicate no abundance differences outside the estimated errors. From a comparison of the derived atmospheric parameters with recent theoretical evolutionary models, we derive distance and age estimates for individual stars. Using kinematical considerations, we conclude that all these objects are `runaway' stars, formed in the Galactic disk and subsequently ejected, possibly by supernovae explosions or dynamical interactions.
PG 0855+294 08 58 21.0 +29 12 12 PG 0934+145 09 37 04.0 +14 18 24 PG 0955+291 09 58 14.4 +28 52 26 PG 1205+228 12 07 57.4 +22 31 47 PG 2219+094 22 21 59.1 +09 37 31 PG 2229+099 22 32 08.5 +10 14 25 PG 2345+241 23 48 22.4 +24 23 06
Equivalent width for the non-diffuse helium and metal lines (PG 0855+294 to PG 2219+094) Line Wavelength of spectral line 0.1nm Species Ionization stage of element --- EW0855 Equivalent width for PG 0855+294 0.1pm A0855 LTE abundances for PG 0855+294 in 12+log(X/H) --- EW0934 Equivalent width for PG 0934+145 0.1pm A0934 LTE abundances for PG 0934+145 in 12+log(X/H) --- EW0955 Equivalent width for PG 0955+291 0.1pm A0955 LTE abundances for PG 0955+291 in 12+log(X/H) --- EW1205 Equivalent width for PG 1205+228 0.1pm A1205 LTE abundances for PG 1205+228 in 12+log(X/H) --- EW2219 Equivalent width for PG 2219+094 0.1pm A2219 LTE abundances for PG 2219+094 in 12+log(X/H) --- Equivalent width for the non-diffuse helium and metal lines (PG 2229+099 and PG 2345+241) Line Wavelength of spectral line 0.1nm Species Ionization stage of element --- EW2229 Equivalent width for PG 2229+099 0.1pm A2229 LTE abundances for PG 2229+099 in 12+log(X/H) --- EW2345 Equivalent width for PG 2345+241 0.1pm A2345 LTE abundances for PG 2345+241 in 12+log(X/H) --- Patricia Bauer CDS 1999 Apr 29 Robert Rolleston <R.Rolleston@Queens-Belfast.AC.UK> J_A+A_347_69.xml HST observations of the very young SMC "blob" N88A J/A+A/347/841 J/A+A/347/841 HST Observations of SMC N88A HST observations of the very young SMC "blob" N88A M Heydari-Malayeri V Charmandaris L Deharveng M R Rosa H Zinnecker Astron. Astrophys. 347 841 1999 1999A&A...347..841H Magellanic Clouds Photometry Stars, early-type dust, extinction HII regions ISM: individual (N 88A) Magellanic Clouds stars: early-type We present the photometry of the 63 brightest stars found in N88 as identified in the finder chart (Fig. 6) of our paper. High-resolution Hubble Space Telescope images have allowed us for the first time to resolve the compact SMC ionized ``blob'' N88A (diameter ~3.5arcsec or 1pc). This very young HII, region, which is hatching from its natal molecular cloud, is heavily affected by absorbing dust associated with the cloud. The interstellar reddening towards N88A is on average A_v_~1.5mag and strikingly rises to more than 3.5mag in a narrow dust band crossing the core of the HII region. Such a high extinction is unprecedented for an HII region in the metal-poor SMC. We present the photometry of some 70 stars lying towards the OB association at the center of which lies N88A. The exciting star(s) of N88A is not detected, due to the heavy extinction. The chronology of star formation is discussed for the whole region.
HST
Photometry of the brightest stars towards N88 Seq Sequential star number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec wideUmag Magnitude in U (F300W) filter mag vmag Magnitude in v (F410W) filter mag bmag Magnitude in b (F467M) filter mag HeII Magnitude in He II (F469N) filter mag ymag Magnitude in y (F547M) filter mag Notes Notes number=1 The capital letters B to H indicate the associated 2 regions presented in Fig.1b. The spectral types and identifications of Wilcots (1994AJ....108.1674W) for some stars are included inside parentheses. Star numbers are indicated in Fig.6. --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1999 Apr 23 Mohammad Heydari-Malayeri <heydari@mesioq.obspm.fr> J_A+A_347_841.xml Photometric analysis of the neglected eclipsing binary system DL Cygni J/A+A/349/515 J/A+A/349/515 DL Cygni ubr differential photometry Photometric analysis of the neglected eclipsing binary system DL Cygni T Borkovits I B Biro Astron. Astrophys. 349 515 1999 1999A&A...349..515B Binaries, eclipsing Photometry stars: binaries: eclipsing stars: individual: DL Cyg stars: fundamental parameters techniques: photometric Relative photometry of DL Cygni versus GSC 3595-0200 in the instrumental system
DL Cyg 21 39 46.5 +48 32 24 GSC 3595-0200 21 39 40.5 +48 29 30
Differential magnitude in v, b and r light HJD Heliocentric Julian Date d Filter Filter designation --- Dmag Differential magnitude in filter "Filter" mag e_Dmag Formal error of "Filter" magnitude mag table3a.tex LaTeX version of table3 (first part) table3b.tex LaTeX version of table3 (second part) table3c.tex LaTeX version of table3 (third part) Patricia Bauer CDS 1999 Aug 10 Tamas Borkovits <borko@electra.bajaobs.hu> J_A+A_349_515.xml Time series analysis of V368 Cephei photometry J/A+A/350/513 J/A+A/350/513 V368 Cep UBVRI time series Time series analysis of V368 Cephei photometry J Kahanpaa L Jetsu L Alha O V Ezhkova K N Grankin T Hackman M A Ibragimov M Kokko V B Kondratiev T Laakso O Lindroos S Yu Mel'nikov P O Nikula J Schultz V S Shevchenko J Torppa I Tuominen J Tyynela J Virtanen Astron. Astrophys. 350 513 1999 1999A&A...350..513K Stars, variable Photometry, UBVRI stars: variables: general stars: individual: (V368 Cep) techniques: photometric Our time series analysis of V368 Cep photometry ascertains the rotation period of 2.74d uniquely. The manifestations of starspot induced luminosity variations in this chromospherically active star include rapid light curve changes and differential rotation of about 3%. We conclude that the single rapidly rotating variable V368 Cep is a high inclination K1V post T Tauri star.
V368 Cep HD 220140 23 19 26.6 +79 00 13
The collected photometry of V368 Cep Set Set number --- HJD Observing time d Umag U magnitude number=1 The standard Johnson UBVRI magnitudes are given, except for SET=3, 4 and 5, which contain magnitude differences between V368 Cep and HD219522 in standard Johnson U and Cousins (RI)_C_. mag Bmag B magnitude number=1 The standard Johnson UBVRI magnitudes are given, except for SET=3, 4 and 5, which contain magnitude differences between V368 Cep and HD219522 in standard Johnson U and Cousins (RI)_C_. mag Vmag V magnitude number=1 The standard Johnson UBVRI magnitudes are given, except for SET=3, 4 and 5, which contain magnitude differences between V368 Cep and HD219522 in standard Johnson U and Cousins (RI)_C_. mag Rmag R magnitude number=1 The standard Johnson UBVRI magnitudes are given, except for SET=3, 4 and 5, which contain magnitude differences between V368 Cep and HD219522 in standard Johnson U and Cousins (RI)_C_. mag Imag I magnitude number=1 The standard Johnson UBVRI magnitudes are given, except for SET=3, 4 and 5, which contain magnitude differences between V368 Cep and HD219522 in standard Johnson U and Cousins (RI)_C_. mag Flare Detected flares --- table5.tex LaTeX version of table 5 Patricia Bauer CDS 1999 Sep 10 Lauri Jetsu <jetsu@gstar.astro.helsinki.fi> J_A+A_350_513.xml Abundances of light elements in metal-poor stars. II. Non-LTE abundance corrections J/A+A/350/955 J/A+A/350/955 Atmospheric parameters in metal-poor stars. II Abundances of light elements in metal-poor stars. II. Non-LTE abundance corrections R G Gratton E Carretta K Eriksson B Gustafsson Astron. Astrophys. 350 955 1999 1999A&A...350..955G J/A+A/314/191 : Atmospheric parameters in metal-poor stars. I (Gratton+, 1996) J/AJ/110/2319 : Abundances in RR Lyrae variables (Clementini+ 1995) Stars, metal-deficient Abundances Models, atmosphere stars: abundances stars: atmospheres stars: population II Sun: abundances We present non-LTE corrections to abundances of Fe, O, Na, and Mg derived from LTE analyses of F-K stars over a broad range of gravities and metal abundances; they were obtained using statistical equilibrium calculations and new model atoms. Line opacity was considered by means of an empirical procedure where it was attributed to a veil of weak Fe I lines; in the case of solar-type dwarfs, results were compared with those obtained using (LTE) mean intensities computed from OSMARCS models. We think that the empirical procedure produces better results for metal-poor stars, while mean intensities should perhaps be preferred for the Sun (where departures from LTE are anyway not very large). Collisions with both electrons and H I atoms were considered. Since cross sections for this second mechanism are very poorly known, we calibrated them empirically by matching observations of RR Lyrae variables at minimum light (discussed in Clementini et al., 1995, Cat. <J/AJ/110/2319>). These stars were selected because non-LTE effects are expected to be larger in these stars than in those usually considered in the study of the chemical evolution of the Galaxy (cool main sequence and red giant branch stars). We found that different non-LTE mechanisms are important for the different species and transitions considered; on the whole, our calculations yielded moderate corrections to LTE abundances for high excitation O lines in warm dwarfs and giants, Na and Mg lines in giants and supergiants, and Fe I lines in F-supergiants (where corrections becomes very large for IR O lines). Non-LTE corrections were found to be negligible in the other cases studied.
Levels for Fe I, O I, Na I and Mg I atoms Ion Ion designation --- Level Level --- E Energy cm-1 Weigth Statistical weight --- Ident Identification --- CrossSec Threshold Cross Section cm+2 Bound-bound transitions Ion Ion designation --- UpperL Upper level --- LowerL Lower level --- Lambda Wavelength nm Abs Absorption oscillator strength --- Einst Einstein factor s-1 Corrections to LTE abundances Ion Ion designation --- [A/H] Abundance [A/H] (logarithmic scale) [Sun] Lambda Wavelength 0.1nm EP Excitation Potential eV EW Equivalent Width 0.1pm C4kK1.5 Correction for models with Teff=4000, logg=1.50 --- C4kK3 Correction for models with Teff=4000, logg=3.00 --- C4kK4.5 Correction for models with Teff=4000, logg=4.50 --- C5kK1.5 Correction for models with Teff=5000, logg=1.50 --- C5kK3 Correction for models with Teff=5000, logg=3.00 --- C5kK4.5 Correction for models with Teff=5000, logg=4.50 --- C6kK1.5 Correction for models with Teff=6000, logg=1.50 --- C6kK3 Correction for models with Teff=6000, logg=3.00 --- C6kK4.5 Correction for models with Teff=6000, logg=4.50 --- C7kK1.5 Correction for models with Teff=7000, logg=1.50 --- C7kK3 Correction for models with Teff=7000, logg=3.00 --- C7kK4.5 Correction for models with Teff=7000, logg=4.50 --- Patricia Bauer CDS 1999 Sep 07 Raffaele Gratton <gratton@mostro.pd.astro.it> J_A+A_350_955.xml Time series analysis of V1794 Cygni long-term photometry J/A+A/351/212 J/A+A/351/212 V1794 UBVR time series Time series analysis of V1794 Cygni long-term photometry L Jetsu J Pelt I Tuominen Astron. Astrophys. 351 212 1999 1999A&A...351..212J J/A+AS/139/513 : 1975-1995 V1794 Cyg UBVRI photometry (Jetsu+, 1999) Stars, variable Photometry, UBVRI stars: individual (V1794 Cyg) stars: variables: general stars: activity techniques: photometric Standard Johnson UBVRI photometry of V1794 Cyg (HD 199178) between 1975 and 1995 is analysed. Instead of the traditional constant period ephemeris, we determine the seasonal periodicities (P_phot_) and the primary and secondary minima epochs (t_min,1_, t_min,2_) of the normalized UBVRI magnitudes using the three stage period analysis (TSPA) and complementary methods.
V1794 Cyg HD 199178 20 53 53.7 +44 23 11
Means and total amplitudes for the modelled UBVR light curves of subsets with number of observing nights (Nnigths) >=7 SET Subset number --- Epoch Observation date yr MUmag Mean U amplitude mag e_MUmag rms uncertainty on MUmag mag AUmag Total U amplitude mag e_AUmag rms uncertainty on AUmag mag MBmag Mean B amplitude mag e_MBmag rms uncertainty on MBmag mag ABmag Total B amplitude mag e_ABmag rms uncertainty on ABmag mag MVmag Mean V amplitude mag e_MVmag rms uncertainty on MVmag mag AVmag Total V amplitude mag e_AVmag rms uncertainty on AVmag mag MRmag Mean R amplitude mag e_MRmag rms uncertainty on MRmag mag ARmag Total R amplitude mag e_ARmag rms uncertainty on ARmag mag The t_min,1_, t_min,2_ and P for the y_norm_ of subsets with Nnigths>=7. SET Subset number --- Nnigths Number of observing nights --- HG Rejections number=1 The rejections are denoted with "r", while the rejections are applied to subsets with Nnigths<10. Finally, rejects the t_min,2_ with S<190 --- Per Period d e_Per rms uncertainty on Per d tmin1 Epoch of the primary minimum in time d e_tmin1 rms uncertainty on tmin1 d tmin2 Epoch of the secondary minimum in time d e_tmin2 rms uncertainty on tmin2 d S Number of times that a secondary minimum t_min_2 was present in the models of 200 bootstrap samples. --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1999 Sep 10 Lauri Jetsu <jetsu@gstar.astro.helsinki.fi> J_A+A_351_212.xml Study of proper motions in the region of the open cluster M67 and membership of stars J/A+AS/100/243 J/A+AS/100/243 Proper motions in M 67 Study of proper motions in the region of the open cluster M67 and membership of stars J -L Zhao K P Tian R S Pan Y P He H M Shi Astron. Astrophys. Suppl. Ser. 100 243 1993 1993A&AS..100..243Z Clusters, open Proper motions membership open clusters and associations: general proper motions Relative proper motions and membership probabilities of 1046 stars in the open cluster M67 are are determined from PDS measurements of 9 plate pairs taken with the double astrograph at the Zo-Se station Shanghai Observatory, which has an aperture of 40cm, a focal length of 6.9m and a scale of 30"/mm. The number of stars with membership probabilities higher than 0.8 and at a distance less than 45' from the field center is 282. The average standard errors of proper motions vary from +/-0.0004"/yr for bright stars in the inner part of the field to some +/-0.0015"/yr for faint stars in the outer part of the cluster. It is shown by a detailed discussion that the proper motions and membership probabilities of the stars determined in this paper are in quite satisfactory agreement wit those obtained by Sanders (1977A&AS...27...89S) or Girard et al. (1989AJ.....98..227G).
M 67 NGC 2682 08 50.4 +11 49
The catalogue of proper motions and membership probabilities in M 67 No Sequential number number=1 Stars 894 and 1024 are BD +12 1926 and BD +12 1927, respectively --- n_No Unexplained note --- Sanders Sanders (1977A&AS...27...89S) identification number --- Xpos X position number=2 Coordinates from PDS measurements on plate 340 cm Ypos Y position number=2 Coordinates from PDS measurements on plate 340 cm Bmag B magnitude number=3 Magnitudes from Sanders (1977A&AS...27...89S) or calculated on the basis of their PDS magnitudes for stars with no magnitude data available in the Sanders' catalogue mag Vmag V magnitude number=3 Magnitudes from Sanders (1977A&AS...27...89S) or calculated on the basis of their PDS magnitudes for stars with no magnitude data available in the Sanders' catalogue mag pmX Proper motion along X direction arcsec/yr pmY Proper motion along Y direction arcsec/yr e_pmX rms uncertainty on pmX arcsec/yr e_pmY rms uncertainty on pmY arcsec/yr P1 Membership probability, this study % P2 Membership probability, Sanders' catalogue (1977A&AS...27...89S) % N Number of measured plate pairs --- James Marcout, Patricia Bauer CDS 1997 Mar 20 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_100_243.xml Spectroscopic observations of radio source identifications from the 1 Jy, S4, and S5 surveys. III. J/A+AS/100/395 J/A+AS/100/395 Spectroscopic observations of radio source ident Spectroscopic observations of radio source identifications from the 1 Jy, S4, and S5 surveys. III. M Stickel H Kuehr Astron. Astrophys. Suppl. Ser. 100 395 1993 1993A&AS..100..395S galaxies: active galaxies: distances and redshifts quasars: general radio continuum: general *** No Description Available ***
Observed 1Jy radio sources Observed S4 radio sources Observed S5 radio sources Object Object name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec m Magnitude of the optical identification mag Type Type of the optical identification --- S_5GHz 5GHz flux Jy s(11-6) two-point spectral index between 11 and 6 cm --- fc References to published Finding Charts --- Names Other names --- Journal of 1Jy identifications Journal of S4 identifications Journal of S5 identifications Object Object name --- Tel Telescope: CA 3.5 = 3.5 m telescope on Calar Alto, Spain CA 2.2 = 2.2 m telescope on Calar Alto, Spain --- Date Observation date --- iTime Total Integration time s Scale Scale of the wavelength calibrated spectra. 0.1nm/pix Scale2 Scale in in red channel for twin Spectrograph 0.1nm/pix Line data for 1Jy identifications Line data for S4 identifications Line data for S5 identifications Object Object name --- z Redshift computed from unweighted z_ind --- Id Element identification --- lam_0 Rest wavelength 0.1nm lam_obs Observed wavelength 0.1nm z_ind Individual redshift --- FWHM FWHM (for emission line) 0.1nm EW Equivalent width (for emission line) 0.1nm u_EW : = uncertain value --- Flux Flux (10-16erg/s/cm2) 10-19W/m2 u_Flux : = uncertain value --- Rem gal = stellar absorption lines of host galaxy abs = intervening absorption lines cal = calibration uncertain due to second order contamination atm = emission lines affected by atmospheric absorption --- Francois Ochsenbein CDS 1993 Nov 12 J_A+AS_100_395.xml IRAS pointed observations data processing J/A+AS/100/473 J/A+AS/100/473 IRAS pointed observations data IRAS pointed observations data processing R Assendorp P R Wesselius Astron. Astrophys. Suppl. Ser. 100 473 1993 1993A&AS..100..473A infrared: general methods: data analysis techniques: image processing We have developed a system to process raw IRAS Pointed Observation (PO) data, using software developed at the Laboratory for Space Research, Groningen, The Netherlands. Several PO's can be coadded into one image. As an example we processed 99 PO's in the Chamaeleon I molecular cloud in to one image for every IRAS band. The list of extracted point sources contains some 300 new IRAS sources, down to a flux level of 21mJy at 12um.
Associated Source List (ASL) RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin F12 Flux at 12um mJy n_F12 When '*' the flux value is in Jy --- SN12 Signal to noise ratio number=2 Signal to noise if the source is found in the PO map, otherwise it is the flux quality from the catalogue(s) mentioned in the corresponding column 'C' --- Cat12 Catalogue in which the flux is listed number=1 P= PO (Pointed Observation) map (Young E.T. et al. 1985, A users's guide to IRAS pointed observation products) F= FSS (Faint Source Survey) (Moshir M. et al. 1989 Explanatory supplement to the IRAS FSS, IPAC preprint 0044) I= IPSC (IRAS Point Source Catalog) (Joint IRAS Science Working Group, 1988, Infrared Astronomical Satellite, Catalogs and Atlasses, Explanatory Supplement, eds Beichman C.A. et al.) --- F25 Flux at 25um mJy n_F25 When '*' the flux value is in Jy --- SN25 Signal to noise ratio number=2 Signal to noise if the source is found in the PO map, otherwise it is the flux quality from the catalogue(s) mentioned in the corresponding column 'C' --- n_SN25 When '*' only the first quality index in the table is reported --- Cat25 Catalogue in which the flux is listed number=1 P= PO (Pointed Observation) map (Young E.T. et al. 1985, A users's guide to IRAS pointed observation products) F= FSS (Faint Source Survey) (Moshir M. et al. 1989 Explanatory supplement to the IRAS FSS, IPAC preprint 0044) I= IPSC (IRAS Point Source Catalog) (Joint IRAS Science Working Group, 1988, Infrared Astronomical Satellite, Catalogs and Atlasses, Explanatory Supplement, eds Beichman C.A. et al.) --- F60 Flux at 60um mJy n_F60 When '*' the flux value is in Jy --- SN60 Signal to noise ratio number=2 Signal to noise if the source is found in the PO map, otherwise it is the flux quality from the catalogue(s) mentioned in the corresponding column 'C' --- n_SN60 When '*' only the first quality index in the table is reported --- Cat60 Catalogue in which the flux is listed number=1 P= PO (Pointed Observation) map (Young E.T. et al. 1985, A users's guide to IRAS pointed observation products) F= FSS (Faint Source Survey) (Moshir M. et al. 1989 Explanatory supplement to the IRAS FSS, IPAC preprint 0044) I= IPSC (IRAS Point Source Catalog) (Joint IRAS Science Working Group, 1988, Infrared Astronomical Satellite, Catalogs and Atlasses, Explanatory Supplement, eds Beichman C.A. et al.) --- F100 Flux at 100um mJy n_F100 When '*' the flux value is in Jy --- SN100 Signal to noise ratio number=2 Signal to noise if the source is found in the PO map, otherwise it is the flux quality from the catalogue(s) mentioned in the corresponding column 'C' --- n_SN100 When '*' only the first quality index in the table is reported --- Cat100 Catalogue in which the flux is listed number=1 P= PO (Pointed Observation) map (Young E.T. et al. 1985, A users's guide to IRAS pointed observation products) F= FSS (Faint Source Survey) (Moshir M. et al. 1989 Explanatory supplement to the IRAS FSS, IPAC preprint 0044) I= IPSC (IRAS Point Source Catalog) (Joint IRAS Science Working Group, 1988, Infrared Astronomical Satellite, Catalogs and Atlasses, Explanatory Supplement, eds Beichman C.A. et al.) --- New Source List (NSL) RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin F12 Flux at 12um mJy SN12 Signal to noise ratio --- F25 Flux at 25um mJy SN25 Signal to noise ratio --- F60 Flux at 60um mJy SN60 Signal to noise ratio --- James Marcout, Simona Mei CDS 1995 Apr 12 UNKNOWN UNKNOWN Keypunched at CDS J_A+AS_100_473.xml General study of group membership. II. Determination of nearby groups J/A+AS/100/47 J/A+AS/100/47 General study of group membership. II. General study of group membership. II. Determination of nearby groups A M Garcia Astron. Astrophys. Suppl. Ser. 100 47 1993 1993A&AS..100...47G catalogs galaxies: clusters: general methods: numerical We present a whole sky catalog of nearby groups of galaxies taken from the Lyon-Meudon Extragalactic Database. From the 78,000 objects in the database, we extracted a sample of 6392 galaxies, complete up to the limiting apparent magnitude B0 = 14.0. Moreover, in order to consider solely the galaxies of the local universe, all the selected galaxies have a known recession velocity smaller than 5500 km/s. Two methods were used in group construction: a Huchra-Geller (1982) derived percolation method and a Tully (1980) derived hierarchical method. Each method gave us one catalog. These were then compared and synthesized to obtain a single catalog containing the most reliable groups. There are 485 groups of a least three members in the final catalog.
Group of galaxies LGG Group number in the Lyon Group of Galaxies (LGG) catalog --- PGC Identification with the PGC name (according to Paturel et al. 1989a,b) number=1 Paturel et al. 1989a, A&AS 80, 299 Paturel et al. 1989b, Extragalactic Data Base Monographs 1, Vol. 1, 2, 3 (PGC) --- Other Identification with an alternative name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 d DEm Declination 1950 arcmin DEs Declination 1950 arcsec T Morphological type coded according to RC3, when it is known number=2 de Vaucouleurs et al. 1991, Third Reference Catalogue of Bright Galaxies (New York: Spinger Verlag) Vol. I, II, III (RC3) --- v Mean heliocentric radial velocity km/s N (3) --- Patricia Bauer CDS 1993 Nov 17 J_A+AS_100_47.xml UBVRI photometry of FKSZ stars. IV. J/A+AS/100/489 J/A+AS/100/489 UBVRI photometry of FKSZ stars. IV. UBVRI photometry of FKSZ stars. IV. G Carrasco P Lpyola Astron. Astrophys. Suppl. Ser. 100 489 1993 1993A&AS..100..489C catalogs reference systems techniques: photometric The paper presents UBVRI photometry, in the Kron-Cousins system, for 117 stars of the Catalog of Fundamental Faint Stars in the declination zone +18-0 deg. The observations were performed from July 1988 to March 1990 with the ESO 0.50-m telescope at the ESO in La Silla, Chile. The results of 24 nights of observations are reported.
UBVRI photometry of the standard stars Name usual name --- HD HD denomination --- CPD CPD denomination --- V V magnitude mag e_V rms uncertainty on V mag B-V B-V color index mag e_B-V rms uncertainty on B-V 0.001mag U-B U-B color index mag e_U-B rms uncertainty on U-B 0.001mag V-R V-R color index mag e_V-R rms uncertainty on V-R 0.001mag R-I R-I color index mag e_R-I rms uncertainty on R-I 0.001mag n number of observations --- Sp spectral type --- UBVRI photometry of the program stars FKSZ FKSZ denomination --- BD BD denomination --- V V magnitude mag u_V uncertainty flag on V --- e_V rms uncertainty on V 0.001mag B-V B-V color index mag u_B-V uncertainty flag on B-V --- e_B-V uncertainty on B-V 0.001mag U-B U-B color index mag u_U-B uncertainty flag on U-B --- e_U-B rms uncertainty on U-B 0.001mag V-R V-R color index mag u_V-R uncertainty flag on V-R --- e_V-R rms uncertainty on V-R 0.001mag R-I R-I color index mag u_R-I uncertainty flag on R-I --- e_R-I rms uncertainty on R-I 0.001mag n number of observation --- Sp spectral type --- James Marcout, Patricia Bauer CDS 1994 May 09 UNKNOWN UNKNOWN The tables have been keypunched at CDS, Strasbourg J_A+AS_100_489.xml CCD astrometry and instrumental Delta-V photometry of wide visual double stars. III. Differential measurements of often observed southern pairs. J/A+AS/100/517 J/A+AS/100/517 CCD astrometry and instrumental Delta-V CCD astrometry and instrumental Delta-V photometry of wide visual double stars. III. Differential measurements of often observed southern pairs. A Van Dessel D Sinachopoulos Astron. Astrophys. Suppl. Ser. 100 517 1993 1993A&AS..100..517V astrometry binaries: visual We present accurate relative positions and instrumental visual (Bessel V) magnitude differences of southern wide star components. The mean accuracy of the angular separation is 0.02 arcsecs, which corresponds to 1.5 micron on the CCD chip, and of magnitude difference 0.007 mag/exposure. The program pairs are targets of the HIPPARCOS mission and they have been observed at least four times in the last 150 yrs.
The observations (epoch: 1992.5) RAh right ascension 2000 h RAm right ascension 2000 min DE- declination sign --- DEd declination 2000 deg DEm declination 2000 arcmin IDS IDS19000 code of the double stars as listed in WDS (Worley and Douglass, 1984) --- Durchm. Durchmusterung designation of the primaries --- Sp1 spectral type of the primary --- Sp2 spectral type of the component B when known --- mA primary magnitude taken from the WDS mag Delta-V observed magnitude difference Delta-V mag e_Delta-V rms uncertainty on Delta-V mag rho angular separation arcsec e_rho rms uncertainty on rho arcsec theta position angle deg e_theta rms uncertainty on theta deg Francois Ochsenbein CDS 1994 Jan 07 D. Sinachopoulos J_A+AS_100_517.xml Simultaneous uvby-beta photometry of SX Phe stars J/A+AS/100/571 J/A+AS/100/571 Simultaneous uvby-beta photometry of SX Simultaneous uvby-beta photometry of SX Phe stars E Rodriguez A Rolland P Lopez De Coca Astron. Astrophys. Suppl. Ser. 100 571 1993 1993A&AS..100..571R delta Scuti photometry variable We present simultaneous uvby beta photometric observations of five SX Phe stars: XX Cyg, CY Aqr, DY Peg, BS Tuc, and SU Crt. The light curves were obtained at Sierra Nevada Observatory, Granada, Spain and European Southern Observatory, La Silla, Chile on 30 nights from 1986 through 1988 and contain 847 points in each of the four uvby colors of the Stromgren photometric system and 542 points in each of the two narrow and wide channels of the H-beta Crawford system.
XX Cyg / uvby CY Aqr / uvby DY Peg / uvby BS Tuc / uvby SU Crt / uvby JD Heliocentric Julian Day day u u magnitude mag v v magnitude mag b b magnitude mag y y magnitude mag XX Cyg / Hbeta CY Aqr / Hbeta DY Peg / Hbeta BS Tuc / Hbeta SU Crt / Hbeta JD Heliocentric Julian Day day H-beta H-beta photometry mag CDS 1993 Feb 09 J_A+AS_100_571.xml Infrared and optical photometry of galaxies in four clusters and of a sample of early-type galaxies. J/A+AS/100/583 J/A+AS/100/583 Infrared and optical photometry of galaxies in Infrared and optical photometry of galaxies in four clusters and of a sample of early-type galaxies. C Boisson F Durret C Balkowski D Proust Astron. Astrophys. Suppl. Ser. 100 583 1993 1993A&AS..100..583B galaxies: clusters: general galaxies: elliptical and lenticular, cD galaxies: photometry infrared: galaxies JHKL' multi-aperture infrared photoelectric photometry is presented here for a sample of galaxies belonging to the Virgo and ABCG 539 clusters. Optical and infrared photometry are also given for members of the Hydra cluster and of the southern extension of the Perseus supercluster. We also give optical photoelectric photometry of 19 early-type (elliptical and S0) field galaxies.
Virgo ABCG 539 Hydra South. extension of Per supercluster NAME Galaxy name --- TYPE Galaxy type --- REMARK '*' flag --- DATE Observation date --- APER Aperture in arcsec arcsec AD log(A/D0) --- J J magnitude (1.24mum) mag u_J Uncertainty flag (:) on J --- H H magnitude (1.63mum) mag u_H Uncertainty flag (:) on H --- K K magnitude (2.19mum) mag u_K Uncertainty flag (:) on K --- Hydra South. extension of Per supercluster NAME Galaxy name --- TYPE Galaxy type --- REMARK '*' flag --- DATE Observation date --- APER Aperture in arcsec arcsec AD log(A/D0) --- B B magnitude mag u_B Uncertainty flag (:) on B --- V V magnitude mag u_V Uncertainty flag (:) on V --- R R magnitude mag u_R Uncertainty flag (:) on R --- I I magnitude mag u_I Uncertainty flag (:) on I --- Early-type galaxies NAME Galaxy name --- TYPE Galaxy morphological type --- REMARK '*' flag --- DATE Observation date --- APER Aperture in arcsec arcsec AD log(A/D0) --- J J magnitude (1.24mum) mag u_J Uncertainty flag (:) on J --- H H magnitude (1.63mum) mag u_H Uncertainty flag (:) on H --- K K magnitude (2.19mum) mag u_K Uncertainty flag (:) on K --- Lp L' magnitude (3.78mum) mag u_Lp Uncertainty flag (:) on L' --- CDS 1993 Feb 10 J_A+AS_100_583.xml Very low mass proper motion members in the Pleiades J/A+AS/100/607 J/A+AS/100/607 Very low mass proper motion members in the Pleiade Very low mass proper motion members in the Pleiades N C Hambly M R S Hawkins R F Jameson Astron. Astrophys. Suppl. Ser. 100 607 1993 1993A&AS..100..607H astrometry open clusters and associations: individual (Pleiades) stars: low-mass, brown dwarfs A proper motion membership list is presented for the lower mass stars in the Pleiades open cluster based on a survey of about a 5 x 5 deg area around the cluster center. Finder charts prepared from an R passband Schmidt plate are given. Photographic R and I photometry is given for all stars; where possible a V magnitude is also listed. The photometry is accurate to about 0.1 m.
The HHJ catalogue HHJ Identification Number --- RAh Right Ascension (Equinox 1950, Epoch 1989.9) h RAm Right Ascension min RAs Right Ascension s DEd Declination (Equinox 1950, Epoch 1989.9) deg DEm Declination arcmin DEs Declination arcsec V Apparent photographic V magnitude. mag R(59F) Apparent photographic R magnitude. mag I(N) Apparent photographic I magnitude. mag mu Total annual proper motion mas/yr PA Position angle E of N of mu number=1 The equatorial proper motions, expressed in mas/yr, can be derived by mu-alpha = mu * sind(PA) mu-delta = mu * cosd(PA) deg CDS 1993 Feb 10 J_A+AS_100_607.xml Evolutionary Sequences of Stellar Models with New Radiative Opacities. II. Z = 0.02 J/A+AS/100/647 J/A+AS/100/647 Evolutionary Sequences of Stellar Models with New Evolutionary Sequences of Stellar Models with New Radiative Opacities. II. Z = 0.02 A Bressan F Fagotto G Bertelli C Chiosi Astron. Astrophys. Suppl. Ser. 100 647 1993 1993A&AS..100..647B Hertzsprung-Russell (HR diagram) stars: abundances stars: evolution stars: imaging stars: interiors A large grid of stellar models computed with the most recent radiative opacities by Iglesias et al. (1992) is presented. The evolutionary tracks have initial masses in the range 0.6 to 120 solar masses and extend from the ZAMS to the beginning of the thermally pulsing regime of the AGB for low and intermediate mass stars, and to the central C-ignition for higher masses. Two smaller samples of stellar models are also presented. The first deals with models of the same chemical composition and opacity but calculated with the classical scheme of mixing. They are meant to provide the necessary tool for discriminating among the two types of mixing. The other sample contains models of the same composition calculated with overshoot and classical radiative opacities by Huebner et al. (1977).
Table 1, M=0.60 Table 1, M=0.70 Table 1, M=0.80 Table 1, M=0.90 Table 1, M=1.00 Table 1, M=1.1 Table 1, M=1.2 Table 1, M=1.3 Table 1, M=1.4 Table 1, M=1.5 Table 1, M=1.6 Table 1, M=1.7 Table 1, M=1.8 Table 1, M=1.9 Table 1, M=2.0 Table 2, M=0.50 Table 2, M=0.55 Table 2, M=0.60 Table 2, M=0.70 Table 2, M=0.80 Table 2, M=0.90 Table 2, M=1.0 Table 2, M=1.1 Table 2, M=1.2 Table 2, M=1.3 Table 2, M=1.4 Table 2, M=1.5 Table 2, M=1.6 Table 2, M=1.7 Table 2, M=2.0 Table 3, M=2.2 Table 3, M=2.5 Table 3, M=3.0 Table 3, M=4.0 Table 3, M=5.0 Table 3, M=6.0 Table 3, M=7.0 Table 3, M=9.0 Table 5, M=2.5 Table 5, M=3.0 Table 5, M=4.0 Table 5, M=5.0 Table 5, M=7.0 Table 5, M=9.0 Age Age of models yr log.L log of total luminosity Sun log.Te log of effective temperature K log.g log of surface gravity cm/s2 log.Tc log of central temperature K log.rho_c log of central density g/cm3 Comp central abundance (by mass) of H or He --- XC central abundance of 12 C --- XO central abundance of 16 O --- Conv fractionary mass of the convective core (inclusive of overshoot) --- Q_disc fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log.L_H log of H luminosity Sun Q1_H fractionary mass of the inner border of the H-rich region --- Q2_H fractionary mass of the outer border of the H-burning region. The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- log.L_He log of He luminosity Sun Q1_He fractionary mass of the inner border of the He-burning region (when greater than zero He-burning is in a shell). The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- Q2_He fractionary mass of the upper border of the He-burning region. The boundary is taken as above. --- log.L_C log of C luminosity Sun log.L_nu log of neutrinos luminosity (absolute value) Sun Q_Tmax fractionary mass of the point where the temperature attains the maximum value --- Table 4, M=12 Table 4, M=15 Table 4, M=20 Table 4, M=30 Table 4, M=40 Table 4, M=60 Table 4, M=100 Table 4, M=120 Table 5, M=12 Table 5, M=15 Table 5, M=20 Age Age of models yr M current value of the Mass Sun log.L log of total luminosity Sun log.Te log of effective temperature K log.g log of surface gravity cm/s2 log.Tc log of central temperature K log.rho_c log of central density g/cm3 Comp central abundance (by mass) of H or He --- XC central abundance of 12 C --- XO central abundance of 16 O --- Conv fractionary mass of the convective core (inclusive of overshoot) --- Q_disc fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log.L_H log of H luminosity Sun Q1_H fractionary mass of the inner border of the H-rich region --- log.L_He log of He luminosity Sun log.Mdot log of absolute value of mass loss rate Sun/yr X_sur surface abundance (by mass) of 1 H --- Y_sur surface abundance (by mass) of 4 He --- XC_sur surface abundance (by mass) of 12 C --- XN_sur surface abundance (by mass) of 14 N --- XO_sur surface abundance (by mass) of 16 O --- table1.tex Table 1, LaTeX table2.tex Table 2, LaTeX table3.tex Table 3, LaTeX table4.tex Table 4, LaTeX table5.tex Table 5, LaTeX CDS 1993 Feb 09 J_A+AS_100_647.xml Classification and statistical properties of galactic H2O masers J/A+AS/101/153 J/A+AS/101/153 Classification and statistical properties of gal Classification and statistical properties of galactic H2O masers F Palagi R Cesaroni G Comoretto M Felli V Natale Astron. Astrophys. Suppl. Ser. 101 153 1993 1993A&AS..101..153P circumstellar matter infrared: ISM infrared: stars ISM: general masers *** No Description Available ***
H2O Masers and IRAS-PSC sources. N Sequential number --- RAh Right Ascension of H2O observations (B1950) h RAm RAm min RAs RAs s DE- Declination Sign --- DEd Declination of H2O observations (B1950) deg DEm DEm arcmin DEs DEs arcsec Name Name of the maser source --- Class Class to which the source is assigned --- GLON Galactic longitude deg GLAT Galactic latitude deg IRAS IRAS name --- dRA R.A. offset H2O - IRAS arcsec dDE Dec. offset H2O - IRAS arcsec Rem Number of associated IRAS sources For non digit character meaning see the description of table1, col 11 in the paper. --- Parameters of H2O Masers. N Sequential number --- n_FLUX Flag : < upper limit * Single component source --- FLAG Flux density of the strongest component in the spectrum Jy H2Oflux Integrated H2O flux Jy pVel Velocity of the peak km/s lVel Velocity of the lowest component km/s hVel Velocity of the highest component km/s FWHM FWHM of the strongest component km/s oVel Offset of the strongest component from the mean velocity, normalized to the emission interval. --- FIR FIR flux integrated over the four IRAS bands. W/m2 Dist Distance kpc MasLum Maser luminosity Sun FIRLum FIR luminosity Sun CDS 1993 Mar 12 J_A+AS_101_153.xml Photoelectric Photometry of field variables. II J/A+AS/101/195 J/A+AS/101/195 Photoelectric Photometry of field variables. I Photoelectric Photometry of field variables. II A M Piersimoni A Di Paolantonio R Burchi R De Santis Astron. Astrophys. Suppl. Ser. 101 195 1993 1993A&AS..101..195P stars: individual (ST Boo, BT Dra, BK Dra, AB Uma, VZ Cnc) *** No Description Available ***
B,V photometry of 4 RR Lyrae of field: ST Boo, BT Dra, BK Dra, AB UMa NAME Variable name --- MJD Julian Day - 2440000 d Phase Phase --- V V mag B-V B-V mag U,B,V photometry of VZ Cnc NAME Variable name --- MJD Julian Day - 2440000 d Phase Phase --- V V mag B-V B-V mag U-B U-B mag CDS 1993 Mar 08 J_A+AS_101_195.xml Wavelengths and transition probabilities of the 3d6-3d54p and 3d54s-3d54p transition arrays of Fe III J/A+AS/101/1 J/A+AS/101/1 Wavelengths and transition probabilities of the Wavelengths and transition probabilities of the 3d6-3d54p and 3d54s-3d54p transition arrays of Fe III J O Ekberg Astron. Astrophys. Suppl. Ser. 101 1 1993 1993A&AS..101....1E atomic data Fe III transition probabilities wavelengths *** No Description Available ***
Wavelength list 59.8-210.5 nm Wavelength list 210.5-812.3 nm Comments Comments on line: see note number=1 The intensities are given first and are in table1: estimates of photographic blackening on a logarithmic scale in table2: marked E when from Edlen and Swings (1942) and G when from Glad (1956) A roman figure following the intensity indicates an affected (a) line and blended (b) line of that iron spectrum. An arabian figure gives the multiplet number from Moore (1952). --- gA gA-values s-1 Lambda(pre) Predicted wavelengths in vacuum (table1) in air (table2) (from energy levels): see note number=2 Predicted wavelengths are calculated from the adopted level energies in table 3 and table4. Observed are from: the present measurement in table1 Edlen and Swings (1942) and Glad (1956) in table2 0.1nm Lambda(obs) Observed wavelengths 0.1nm Sigma Predicted wavenumbers cm-1 lower Designation of lower level in combination --- upper Designation of upper level in combination --- Level list of 3d6 and 3d5 4s Level list of 3d5 4p Designation Designations of level --- Energy Level energies cm-1 No. Number of combinations with the level --- Patricia Bauer CDS 1993 Sep 28 J_A+AS_101_1.xml Redshifts of southern rich clusters J/A+AS/101/259 J/A+AS/101/259 Redshifts of southern rich clusters Redshifts of southern rich clusters M Galli A Cappi P Focardi L Gregorini G Vettolani Astron. Astrophys. Suppl. Ser. 101 259 1993 1993A&AS..101..259G galaxies: clusters: general galaxies: distances and redshifts We present radial velocities of 53 galaxies lying in the direction of 13 southern ACO rich clusters (Abell et al 1989). The observations were carried out with the 1.5 m ESO telescope. The spectra have a wavelength range from 3800 to 6800 A with a resolution of ~12 A. For each galaxy we present accurate optical position and finding chart. The table gathers the results of three publications: (1) Radial velocities of 13 southern rich clusters Vettolani G., Cappi A., Chincarini G., Focardi P., Garilli B., Gregorini L., Maccagni D. <Astron. Astrophys. Suppl. Ser. 79, 147 (1989)> =1989A&AS...79..147V (2) Redshifts of southern ch clusters Cappi A., Focardi P., Gregorini L., Vettolani G. <Astron. Astrophys. Suppl. Ser. 88, 349 (1991)> =1991A&AS...88..349C (3) Galli M., Cappi A., Focardi P., Gregorini L., Vettolani G. <Astron. Astrophys. Suppl. Ser. 101, 259 (1993)> =1993A&AS..101..259G
Results from the three papers Abell Abell number --- N Galaxy number in cluster (cf identification charts) --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec Vh Heliocentric velocity km/s e_Vh mean error on Vh km/s table.tex plain TeX version CDS 1993 Feb 17 J_A+AS_101_259.xml Grids of stellar models. III. From 0.8 to 120 Msolar at Z=0.004 J/A+AS/101/415 J/A+AS/101/415 Grids of stellar models. III. From 0.8 to 120 Grids of stellar models. III. From 0.8 to 120 Msolar at Z=0.004 C Charbonnel G Meynet A Maeder G Schaller D Schaerer Astron. Astrophys. Suppl. Ser. 101 415 1993 1993A&AS..101..415C Hertzsprung-Russell (HR diagram) stars: evolution *** No Description Available ***
M=120, Z=0.004, with overshooting, standard mass loss M=85, Z=0.004, with overshooting, standard mass loss M=60, Z=0.004, with overshooting, standard mass loss M=40, Z=0.004, with overshooting, standard mass loss M=25, Z=0.004, with overshooting, standard mass loss M=20, Z=0.004, with overshooting, standard mass loss M=15, Z=0.004, with overshooting, standard mass loss M=12, Z=0.004, with overshooting, standard mass loss M=9, Z=0.004, with overshooting, standard mass loss M=7, Z=0.004, with overshooting, standard mass loss M=5, Z=0.004, with overshooting, standard mass loss M=4, Z=0.004, with overshooting, standard mass loss M=3, Z=0.004, with overshooting, standard mass loss M=2.5, Z=0.004, with overshooting, standard mass loss M=2, Z=0.004, with overshooting, standard mass loss M=1.7, Z=0.004, with overshooting, standard mass loss M=1.5, Z=0.004, with overshooting, standard mass loss M=1.25, Z=0.004, with overshooting, standard mass loss M=1.25, Z=0.004, no overshooting, standard mass loss M=1, Z=0.004, no overshooting, standard mass loss M=0.9, Z=0.004, no overshooting, standard mass loss M=0.8, Z=0.004, no overshooting, standard mass loss NB number of selected point --- Age age yr Mass actual mass in solar masses Sun logL log(luminosity) in solar units Sun logTe log(effective temperature) K X H surface abundance (mass fraction) --- Y He surface abundance (mass fraction) --- C12 12C surface abundance (mass fraction) --- C13 13C surface abundance (mass fraction) --- N14 14N surface abundance (mass fraction) --- O16 16O surface abundance (mass fraction) --- O17 17O surface abundance (mass fraction) --- O18 18O surface abundance (mass fraction) --- Ne20 20Ne surface abundance (mass fraction) --- Ne22 22Ne surface abundance (mass fraction) --- QCC core mass fraction --- logTu log(uncorrected Teff) (WR stars only) K logMdot log(mass loss rate) Sun/yr log(rho_c) log(central density) g/cm3 logTc log(central temperature) K Xc H central abundance (mass fraction) --- Yc He central abundance (mass fraction) --- C12c 12C central abundance (mass fraction) --- C13c 13C central abundance (mass fraction) --- N14c 14N central abundance (mass fraction) --- O16c 16O central abundance (mass fraction) --- O17c 17O central abundance (mass fraction) --- O18c 18O central abundance (mass fraction) --- Ne20c 20Ne central abundance (mass fraction) --- Ne22c 22Ne central abundance (mass fraction) --- Patricia Bauer CDS 1993 Sep 27 J_A+AS_101_415.xml Simultaneous uvby-beta photometry of GP Andromedae J/A+AS/101/421 J/A+AS/101/421 Simultaneous uvby-beta photometry of GP Simultaneous uvby-beta photometry of GP Andromedae E Rodriguez A Rolland P Lopez De Coca Astron. Astrophys. Suppl. Ser. 101 421 1993 1993A&AS..101..421R delta Scuti stars: individual (GP And) stars: oscillations *** No Description Available ***
Magnitude differences GP And-HD 5213 in the standard uvby system versus Heliocentric Julian Day JDHel Heliocentric Julian Day d v in standard uvby system mag b-y in standard uvby system mag m1 = (v-b) - (b-y) mag c1 = (u-v) - (v-b) mag Standard H-beta values of GP And versus Heliocentric Julian Day JDhel Heliocentric Julian Day d Hbeta Standard H-beta index mag CDS 1993 Mar 12 J_A+AS_101_421.xml Spectroscopic observations of the galaxy cluster A 3571 (SC 1344-325) J/A+AS/101/475 J/A+AS/101/475 Spectroscopic observations of A3571 Spectroscopic observations of the galaxy cluster A 3571 (SC 1344-325) H Quintana R de Souza Astron. Astrophys. Suppl. Ser. 101 475 1993 1993A&AS..101..475Q Clusters, galaxy Radial velocities galaxies: clusters: general galaxies: velocities X-ray clusters Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.
Galaxy velocities in SC 1344-325 = A 3571 Name Object name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec HV Heliocentic velocity km/s Nline Number of lines measured in each spectrum --- Qual Quality comment --- Tel Telescope number=1 3.6OPT: OPTOPUS T1IT: CTIO 1m E1IT: ESO 1.5m T4V: CTIO 4m --- Group Subclustering group --- Note Notes --- Patricia Bauer CDS 1997 Nov 18 UNKNOWN UNKNOWN OCR by LEDA team (Lyon Observatory) for the name, position and velocity columns, proof-read by H. Andernach in December 1994 (LEDA ref no. 24257). The other columns were added at CDS. J_A+AS_101_475.xml COYOTES I. Multisite UBVRI photometry of 24 pre-main-sequence stars of the Taurus-Auriga cloud J/A+AS/101/485 J/A+AS/101/485 COYOTES I. Multisite UBVRI photometry of 24 COYOTES I. Multisite UBVRI photometry of 24 pre-main-sequence stars of the Taurus-Auriga cloud J Bouvier S Cabrit M Fernandez E L Martin J M Matthews Astron. Astrophys. Suppl. Ser. 101 485 1993 1993A&AS..101..485B stars: activity stars: pre-main sequence stars: rotation *** No Description Available ***
UBVRI photometry Name Name --- HBC HBC name (Lick Obs. Bull. 1111) --- JD Julian Day (JD -2400000) d V V magnitude mag B-V B-V colour mag U-B U-B colour mag V-R V-R colour mag V-I V-I colour mag Francois Ochsenbein CDS 1993 Nov 30 J_A+AS_101_485.xml Near-infrared and sub-millimeter photometry of carbon stars J/A+AS/101/513 J/A+AS/101/513 Near-infrared and sub-millimeter photometry Near-infrared and sub-millimeter photometry of carbon stars M A T Groenewegen T De Jong F Baas Astron. Astrophys. Suppl. Ser. 101 513 1993 1993A&AS..101..513G circumstellar matter infrared: stars radio continuum: stars stars: carbon *** No Description Available ***
Sub-millimeter AFGL AFGL Number --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Ident Identifier number=1 References to the carbon star nature. The numbers refer to the GCCCS (Stephenson 1989). Other references are labelled as: MSa = Merrill & Stein (1976a), MSb = Merrill & Stein (1976b), CK = Cohen & Kuhi (1977), Jo = Jones et al. (1978), 3M = star shows the characteristic 3mum feature (Groenewegen et al. In preparation), SiC = LRS spectrum shows the silicon carbide feature. LRS = LRS spectrum does not show SiC but is very similar to other extremely red carbon stars like AFGL 190 or AFGL 3068. --- l_F100 '<' for upper limit on F100 --- F100 IRAS 100mu flux Jy e_F100 m.e. on F100 Jy F450 Flux at 450mum mJy e_F450 m.e. on F450 mJy l_F600 '<' for upper limit on F600 --- F600 Flux at 600mum mJy e_F600 m.e. on F600 mJy F800 Flux at 800mum mJy e_F800 m.e. on F800 mJy F1100 Flux at 1100mum mJy e_F1100 m.e. on F1100 mJy Group Group designation of Groenewegen et al. 1992 --- JHKLM photometry IRAS IRAS name --- Ident Reference to the Carbon nature number=1 See above --- J J magnitude mag e_J m.e. on J mag H H magnitude mag e_H m.e. on H mag K K magnitude mag e_K m.e. on K mag L L magnitude mag e_L m.e. on L mag M M magnitude mag e_M m.e. on M mag [12-25] IRAS index 12/25 mum mag Tel Telescope --- Ref References number=2 Ground based NIR photometry before 1987 is referred to as Ge, the Gezari et al. (1987) catalog. Later work is labelled as follows: Me = Meadows et al. (1987), E87 = Epchtein et al. (1987), LB = Le Bertre (1988), E90 = Epchtein et al. (1990), Jo = Jones et al. (1990). Recently, some stars have independently been observed in the infrared by Fouque et al. (1992) and Guglielmo et al. (1992). These references are labelled as Fo and Gu, respectively. --- Group Group designation of Groenewegen et al. 1992 --- Francois Ochsenbein CDS 1993 Mar 12 J_A+AS_101_513.xml Optical polarization of 1000 stars within 50 pc from the Sun J/A+AS/101/551 J/A+AS/101/551 Optical polarization of 1000 stars Optical polarization of 1000 stars within 50 pc from the Sun J L Leroy Astron. Astrophys. Suppl. Ser. 101 551 1993 1993A&AS..101..551L dust, extinction polarization solar neighborhood *** No Description Available ***
The catalogue HD star identification (HD number) --- GLON Galactic longitude deg GLAT Galactic latitude deg D Distance pc u_D Uncertainty flag (:) on D --- P Polarization degree, in units of 0.001 % 10-5 DP Uncertainty on the polarization degree, in the same unit 10-5 Ref1 Two first letters of the name of the author who has published the polarization data; the detailed references are provided in the original paper. --- Ref2 other references for the same star number=1 other references are in order of decreasing polarimetric accuracy. --- Ref3 other references for the same star number=1 other references are in order of decreasing polarimetric accuracy. --- Ref4 other references for the same star number=1 other references are in order of decreasing polarimetric accuracy. --- CDS 1993 Mar 12 J_A+AS_101_551.xml Four-colour photometry of eclipsing binaries. XXXV. Light curves of GG Lupi: Young metal-deficient B stars. J/A+AS/101/563 J/A+AS/101/563 uvby photometry of GG Lup Four-colour photometry of eclipsing binaries. XXXV. Light curves of GG Lupi: Young metal-deficient B stars. J V Clausen J M Garcia A Gimenez B E Helt L P R Vaz Astron. Astrophys. Suppl. Ser. 101 563 1993 1993A&AS..101..563C binaries: eclipsing photometry stars: individual (GC Lup, HR 5668, HR 5696, HR 5724) *** No Description Available ***
*Magnitude differences GG Lup - HR5696 in the instrumental system (ubvy) INN internal night number --- HJD_i 2440000 - HJD (integer part) d HJD_d 2440000 - HJD (decimal part) d Phase phase calculated from linear ephemeris 2446136.73980 + 1.84960 E --- ymag y magnitude mag (b-y) (b-y) colour mag m1 m1 magnitude mag c1 c1 magnitude mag bmag b magnitude mag vmag v magnitude mag umag u magnitude mag Patricia Bauer CDS 1993 Oct 14 J_A+AS_101_563.xml The Exciting Sources of Herbig-Haro objects. I. A Catalogue of 1-20um observations J/A+AS/101/59 J/A+AS/101/59 1-20um observations of Herbig-Haro objects The Exciting Sources of Herbig-Haro objects. I. A Catalogue of 1-20um observations S Molinari R Liseau D Lorenzetti Astron. Astrophys. Suppl. Ser. 101 59 1993 1993A&AS..101...59M catalogs infrared radiation photometry stars: circumstellar matter stars: mass-loss stars: pre-main sequence For 58 exciting sources of Herbig-Haro objects/jets (HHES) we present a catalogue of photometric data for the infrared spectral bands JHKLMNQ (1-20 um). This catalog is based on our own observations and published information available up to May 1992. For each source, these data are presented in chronological order. In addition to the broad-band data, narrow-band N(8-13 um) photometric data are also provided. The flux calibration for each observational equipment is explicitly noted as the diaphragm sizes are used. The same kind of information for the established members of the FU Ori class is complementing the HHES catalogue. The frequency of observations and the photometric quality of the catalogued data are shortly discussed.
HHES and FUORs summary N Running number (FUORs start with FU) --- Note A * indicates a note (see below) --- Name Source name(s) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec r_pos Reference of position --- HH Designation of the associated HH/jet --- r_HH Reference of HH --- D Distance pc u_D Uncertainty flag (:) on D --- r_D Reference of D --- IRAS Identification of the associated IRAS source --- r_IRAS Reference of IRAS association --- L Bolometric Luminosity of the HHES in solar units Sun r_L Reference of L --- CO Associated molecular outflow (CO) --- r_CO Reference(s) for CO --- Near infrared photometry (tables 2+3) N Running number as coded in the paper. --- n_date Date flag, as: < if the date of the observation is not known but it is less than the one which is given. * the date of the observation is uncertain and one should refer to the paper for details. --- Year Year of the observation. yr Month Month of the observation. ( 0 if unknown) --- Day Day of the observation. ( 0 if unknown) --- h Hour of the observation. ( 0 if unknown) --- min Minute of the observation. ( 0 if unknown) --- r_obs Number of the reference paper in which the observation is published, --- r_pho Number of the reference paper where data about employed photometric systems can be found (0 if no information available) --- lambda Wavelength expressed in microns um Unit Code which identify the units in which data are presented. Coding is as follows: "MA" if data is a magnitude. "ML" if data is a lower limit magnitude. "JY" if data is given in Jansky. "JL" if data is an upper limit in Jansky "MJ" if data is given in milliJansky "W8" if data is given in units of 10^-14 Watts/m2/um --- Value Data expressed in units defined above, or upper limits for "ML" or "JL" Unit --- e_Value Error on Value in units defined above. For "ML" or "JL" Unit, e_Value gives the number of sigma (if known) of the limit. --- n_diaph Code to give informations about the diaphragm used, and may assume the following values: < diaphragm diameter is an upper limit > diaphragm diameter is a lower limit R diaphragm is rectangular V diaphragm diameter is known within a range --- diaph Diaphragm dimensions in ARCSEC (0 when unknown); it has the following meaning according to n_diaph: blank, "<" or ">" : radius of the circular diaphragm. "R" the integer and the decimal part of this number are the alfa and delta dimension of the diaphragm. "V" the integer and the decimal part of this number are respectively the lower and the upper limit of the range. arcsec CDS 1993 Apr 28 J_A+AS_101_59.xml Walraven photometry of eight cataclysmic variables J/A+AS/101/87 J/A+AS/101/87 Walraven photometry of eight cataclysmic Walraven photometry of eight cataclysmic variables A Hollander H Kraakman J Van Paradijs Astron. Astrophys. Suppl. Ser. 101 87 1993 1993A&AS..101...87H accretion, accretion disks novae, cataclysmic variables *** No Description Available ***
VBLUW fluxes BV Cen VBLUW fluxes HL Aqr VBLUW fluxes V426 Oph VBLUW fluxes V603 Aql VBLUW fluxes V2051 Oph VBLUW fluxes V3885 Sgr VBLUW fluxes VY Scl VBLUW fluxes WW Cet BJED BJED - 2447000.00 number=1 Barycentric corrected Julian Ephemeris Date d V Flux in V-band number=2 Bad integrations have a value of -99. mJy B Flux in B-band number=2 Bad integrations have a value of -99. mJy L Flux in L-band number=2 Bad integrations have a value of -99. mJy U Flux in U-band number=2 Bad integrations have a value of -99. mJy W Flux in V-band number=2 Bad integrations have a value of -99. mJy CDS 1993 Feb 11 J_A+AS_101_87.xml Observations of the Sun during 1990-1992 with the astrolabe of Santiago J/A+AS/102/11 J/A+AS/102/11 Observations of the Sun during 1990-1992 with the Observations of the Sun during 1990-1992 with the astrolabe of Santiago F Noel Astron. Astrophys. Suppl. Ser. 102 11 1993 1993A&AS..102...11N astrolabe observations solar positions and semi-diameter *** No Description Available ***
Sun observations at 30 deg zenith distance Sun observations at 60 deg zenith distance date Date (year-1900,month,day) --- MJD Modified julian day d EUB Zenith distance residual east upper border arcsec ELB Zenith distance residual east lower border arcsec WLB Zenith distance residual west lower border arcsec WUB Zenith distance residual west upper border arcsec dAlpha dAlpha = Right ascension (O-C) s e_dAlpha Sigma of dAlpha s Y Y=Declination (O-C) + Zenith distance (Observed-Adopted). arcsec dD dD=Sun semi-diameter (O-C) arcsec e_dD Sigma of dD and Y arcsec DR Observed Sun semi-diameter reduced to AU. arcsec Patricia Bauer CDS 1993 Sep 28 J_A+AS_102_11.xml An objective-prism survey of emission-line objects in M 31. J/A+AS/102/251 J/A+AS/102/251 An objective-prism survey of emission-line An objective-prism survey of emission-line objects in M 31. N Meyssonnier J Lequeux M Azzopardi Astron. Astrophys. Suppl. Ser. 102 251 1993 1993A&AS..102..251M galaxies: individual (M 31) galaxies: stellar content HII regions planetary nebulae: general stars: Wolf-Rayet surveys Using GRENS plates taken at the Canada-France-Hawaii telescope, we have searched almost the whole extent of M 31 for small- diameter objects with strong emission lines. Most are planetary nebulae candidates, but there are also many Wolf-Rayet star candidates and small HII regions or compact parts of large HII regions. A catalogue is presented with a cross-identification with previous catalogues. Many new planetary nebulae and Wolf-Rayet candidates are found. Their distribution is compared with those of other tracers in M 31. In particular the distribution of planetary nebulae candidates is compared with that of the integrated blue light and we confirm the result obtained by Jacoby (1980) and Ciardullo et al. (1989): the number of planetary nebulae per unit total luminosity is a constant throughout the disk of M 31. The Wolf-Rayet star candidates are concentrated in the well-known ring of star formation; their total number is estimated as 300 within the limit of detection of the deepest existing surveys, but this may still be an underestimate of the true number.
catalogue of 1312 emission-line objects in M31 doubtful candidates emission-line objects N Running number --- flag existence flag, as: blank sure : doubtful :: very doubtful --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Npos number of position measurements --- u_Npos Uncertainty flag on Npos, as blank coherent measurements : one measurement doubtful or impossible --- Names other identifications number=1 the following acronyms are used: BA = Baade W.,Arp H.: 1964,ApJ 139, 1027 D = Crampton D., Cowley A.P.,Schade D.,Chayer P.: 1985,ApJ 288, 494 DDB = d'Odorico S.,Dopita M.A.,Benvenuti P.: 1980, A&AS 40, 67 F = Ford H.C., Jenner D.C.: 1975,ApJ 202, 365 Ford H.C., Jacoby G.H.: 1978, ApJS 38, 351 Lawrie D.G., Ford H.C.: 1982,ApJ 256, 120 Nolthenius R., Ford H.C.: 1987,ApJ 317, 62 Ciardullo R.,Jacoby G.H., Ford H.C., Neill J.D.: 1989,ApJ 339, 53 H = Crampton D., Cowley A.P.,Schade D.,Chayer P.: 1985,ApJ 288, 494 IT = Moffat A.F.J., Shara M.M.: 1987, ApJ 320, 266 MS = Moffat A.F.J., Shara M.M.: 1983, ApJ 273, 544 OB = Massey P., Armandroff T.E., Conti P.S.: 1986,AJ 92, 1303 WB = Walterbos R.A.M., Braun R.: 1992,A&AS 92, 625 --- Nature possible nature of the objects (2) (if followed by "?", doubtful nature) --- CDS 1993 Jun 07 J_A+AS_102_251.xml Highly-excited levels of Fe I obtained from laboratory and solar Fourier transform and grating spectra. II. Laboratory and solar identifications J/A+AS/102/269 J/A+AS/102/269 Highly-excited levels of Fe I obtained from Highly-excited levels of Fe I obtained from laboratory and solar Fourier transform and grating spectra. II. Laboratory and solar identifications G Nave S Johansson Astron. Astrophys. Suppl. Ser. 102 269 1993 1993A&AS..102..269N atomic data infrared: general line: identification ultraviolet: general *** No Description Available ***
Fe I lines from 4941.6 to 170.1nm I Intensity (laboratory data)(2) --- FWHM Full width at half maximum of line in FT spectra (laboratory data) 0.001cm-1 Lambda Wavelength (laboratory data) Lambda(air) for lambda > 200nm Lambda(vac) for lambda < 200nm 0.1nm Sigma Wavenumber (laboratory data) cm-1 o-c Difference between observed wavenumber (wavelength below 306 nm) and that derived from the energy levels in paper 1 0.001cm-1 Transition See note 5 --- bl. Species of blended line. Lines marked `G' are blended with a ghost. --- Lambda_Sun Decimal part of wavelength in solar spectrum number=6 Is specified either as wavelength or wavenumber. Solar data is taken from: Geller (1992) 2000 cm-1 < sigma < 4788 cm-1 Biemont et al.(1985) 4788 cm-1 < sigma < 8375 cm-1 Delbouille et al.(1981) 4788 cm-1 < sigma < 8375 cm-1 Livingston and Wallace (1991) 4788 cm-1 < sigma < 8375 cm-1 Swensson et al. (1970) 8375 cm-1 < sigma < 11100 cm-1 Pierce & Breckinridge (1975) 11100 cm-1 < sigma < 32650 cm-1 Moore et al. (1966) 11100 cm-1 < sigma < 32650 cm-1 Moore et al. (1982) 32650 cm-1 < sigma < 47500 cm-1 Moore et al. (1992) sigma > 47500 cm-1 0.1nm Sigma_Sun Decimal part of wavenumber in solar spectrum number=6 Is specified either as wavelength or wavenumber. Solar data is taken from: Geller (1992) 2000 cm-1 < sigma < 4788 cm-1 Biemont et al.(1985) 4788 cm-1 < sigma < 8375 cm-1 Delbouille et al.(1981) 4788 cm-1 < sigma < 8375 cm-1 Livingston and Wallace (1991) 4788 cm-1 < sigma < 8375 cm-1 Swensson et al. (1970) 8375 cm-1 < sigma < 11100 cm-1 Pierce & Breckinridge (1975) 11100 cm-1 < sigma < 32650 cm-1 Moore et al. (1966) 11100 cm-1 < sigma < 32650 cm-1 Moore et al. (1982) 32650 cm-1 < sigma < 47500 cm-1 Moore et al. (1992) sigma > 47500 cm-1 cm-1 I Intensity (solar data) --- Comments See note 7 --- Patricia Bauer CDS 1993 Oct 06 J_A+AS_102_269.xml Grids of stellar models. IV. From 0.8 to 120 M_solar at Z=0.040 J/A+AS/102/339 J/A+AS/102/339 Grids of stellar models. IV. From 0.8 to 120 Grids of stellar models. IV. From 0.8 to 120 M_solar at Z=0.040 D Schaerer C Charbonnel G Meynet A Maeder G Schaller Astron. Astrophys. Suppl. Ser. 102 339 1993 1993A&AS..102..339S Hertzsprung-Russell (HR diagram) stars: evolution *** No Description Available ***
M=120, z=0.040 with overshooting standard mass loss M=85, z=0.040 with overshooting standard mass loss M=60, z=0.040 with overshooting standard mass loss M=40, z=0.040 with overshooting standard mass loss M=25, z=0.040 with overshooting standard mass loss M=20, z=0.040 with overshooting standard mass loss M=15, z=0.040 with overshooting standard mass loss M=12, z=0.040 with overshooting standard mass loss M=9, z=0.040 with overshooting standard mass loss M=7, z=0.040 with overshooting standard mass loss M=5, z=0.040 with overshooting standard mass loss M=4, z=0.040 with overshooting standard mass loss M=3, z=0.040 with overshooting standard mass loss M=2.5, z=0.040 with overshooting standard mass loss NB number of selected point --- Age age yr Mass actual mass in solar masses Sun logL log(luminosity) in solar units Sun logTe log(effective temperature) K X H surface abundance (mass fraction) --- Y He surface abundance (mass fraction) --- C12 12C surface abundance (mass fraction) --- C13 13C surface abundance (mass fraction) --- N14 14N surface abundance (mass fraction) --- O16 16O surface abundance (mass fraction) --- O17 17O surface abundance (mass fraction) --- O18 18O surface abundance (mass fraction) --- Ne20 20Ne surface abundance (mass fraction) --- Ne22 22Ne surface abundance (mass fraction) --- QCC core mass fraction --- logTu log(uncorrected Teff) (WR stars only) K logMdot log(mass loss rate) Sun/yr log(rho_c) log(central density) g/cm3 logTc log(central temperature) K Xc H central abundance (mass fraction) --- Yc He central abundance (mass fraction) --- C12c 12C central abundance (mass fraction) --- C13c 13C central abundance (mass fraction) --- N14c 14N central abundance (mass fraction) --- O16c 16O central abundance (mass fraction) --- O17c 17O central abundance (mass fraction) --- O18c 18O central abundance (mass fraction) --- Ne20c 20Ne central abundance (mass fraction) --- Ne22c 22Ne central abundance (mass fraction) --- Patricia Bauer CDS 1993 Sep 29 J_A+AS_102_339.xml A Catalogue of Li abundances and equivalent widths in a sample of galactic C-stars J/A+AS/102/361 J/A+AS/102/361 A Catalog of Li abundances and equivalent widths A Catalogue of Li abundances and equivalent widths in a sample of galactic C-stars H M J Boffin C Abia J Isern R Rebolo Astron. Astrophys. Suppl. Ser. 102 361 1993 1993A&AS..102..361B stars: abundances stars: late-type *** No Description Available ***
Li abundances and equivalent widths of galactic C-stars VS_Name VS designation --- TMSS_Name TMSS designation --- day date of observation, day/month/year "DD/MM/YY" Period period of the star d W(Li) Li line equivalent width 0.1pm u_W(Li) A ? means that the given data is poor --- l_A(Li) Limit flag on A(Li) --- A(Li) 12+log(N(Li)/N(H)) Li abundance --- u_A(Li) A ? means that the given data is poor --- note peculiarity of the star --- Patricia Bauer CDS 1993 Sep 30 J_A+AS_102_361.xml Colour magnitude diagram for the globular cluster M13 J/A+AS/102/397 J/A+AS/102/397 Colour magnitude diagram of M13 Colour magnitude diagram for the globular cluster M13 M D Guarnieri A Bragaglia F Fusi Pecci Astron. Astrophys. Suppl. Ser. 102 397 1993 1993A&AS..102..397G Clusters, globular Colors Photometry, CCD color-magnitude diagrams (HR diagram) globular clusters: individual (M 13) photometry: CCD stars: evolution Two overlapping regions of M13 were observed on April 24, 1989 at the Loiano Observatory with a CDCD camera. A Colour-Magnitude diagram down to the main sequence was derived, as a preliminary search for the blue Horizontal Branch stars in this cluster.
M 13 NGC 6205 C 1639+365 16 41 41.4 +36 27 37
*B, B-V and positions for 3532 stars in M13 Num Identification Number --- Bmag B magnitude (not Vmag, si "History" section) mag B-V B-V colour mag X X position (increases to West, 0.5"/pix) pix Y Y position (increases to South, 0.5"/pix) pix Patricia Bauer CDS 1993 Oct 14 UNKNOWN UNKNOWN * 17-Jun-1999: Thanks to a note from Wayne Osborn, and a confirmation by Angela Bragaglia, the magnitude listed was relabelled to Bmag, instead of Vmag. J_A+AS_102_397.xml Delta(n) <= 2 allowed transitions of neutral sulphur within the visible and infrared spectral ranges J/A+AS/102/435 J/A+AS/102/435 Delta Delta(n) <= 2 allowed transitions of neutral sulphur within the visible and infrared spectral ranges E Biemont P Quinet C J Zeippen Astron. Astrophys. Suppl. Ser. 102 435 1993 1993A&AS..102..435B atomic data atomic processes Sun: abundances *** No Description Available ***
Configurations selected for the present SST and HFR calculations in S I Mode Calculation mode (SST or HFR) --- EP Even parity configuration --- OP Odd parity configuration --- HFR fitted parameters (even configurations) HFR fitted parameters (odd configurations) Conf. Configuration --- Param. Parameter --- Fit Fitted value cm-1 Fit/HFR Fitted-HFR ratio --- n_Fit/HFR When f, fixed value --- Excitation energies and fine-structure splittings Config Configuration --- Level Level --- E(obs) Observed excitation energy cm-1 DeltaE(obs) Observed fine-structure splitting cm-1 DeltaE(cal) Calculed present fine-structure splitting cm-1 TEC Semi-empirical corrections to calculated non-relativistic energies cm-1 Calculated HFR energy level (even configuration Calculated HFR energy level (odd configuration) Conf Configuration --- Level Level --- E(calc) HFR energy level cm-1 Delta E(obs) - E(calc) cm-1 Comp LS coupling composition: contributions >= 5% only are given % Calculated oscillator strengths (3p3(4S)nl - 3p3(4S)n'l') Calculated oscillator strengths (3p3 (2D)nl - 3p3(2D)n'l') Transition Transition --- Lambda Wavelength calculated with the levels of Martin et al. (1990) 0.1nm HFR Calculated oscillator strength (log gf) obtained with HFR method --- n_HFR Cancellation factor (CF) *, as defined by Cowan (1981) number=1 A small value indicates strong cancellation effect. The starred transitions are those for which CF<=0.02 --- SST Calculated oscillator strength (log gf) obtained with SST method --- n_SST When +, the length and velocity results differ by more than a factor of two --- lg1 Oscillator strength (log gf) from other work --- r_lg1 Reference to result lg1 number=2 a: Kurucz R.L. & Peytremann E., Smith. Astron. Obs. Spec. Report 362 (1975) b: Lambert D.L. & Warner B., MNRAS 138, 181 (1968) c: Biemont E. & Grevesse N., ADNDT 12, 217 (1973) d: Lambert D.L. & Luck R.E., MNRAS 183, 79 (1978) e: Aymar M., NIM 110, 211 (1973) f: Aymar M., Physica 66, 364 (1973) g: Wiese W. L. et al., (1969) h: Foster E.W., Proc. Phys. Soc. London 90, 275 (1967) i: Bridges J.M. & Wiese W.L., Phys. Rev. A159, 31 (1967) k: Miller M.H., Wilkerson T.D., Roig R.A. & Bengston R.D., Phys. Rev. A9, 2312 (1974) --- lg2 Oscillator strength (log gf) from other work --- r_lg2 Reference to result lg2 number=2 a: Kurucz R.L. & Peytremann E., Smith. Astron. Obs. Spec. Report 362 (1975) b: Lambert D.L. & Warner B., MNRAS 138, 181 (1968) c: Biemont E. & Grevesse N., ADNDT 12, 217 (1973) d: Lambert D.L. & Luck R.E., MNRAS 183, 79 (1978) e: Aymar M., NIM 110, 211 (1973) f: Aymar M., Physica 66, 364 (1973) g: Wiese W. L. et al., (1969) h: Foster E.W., Proc. Phys. Soc. London 90, 275 (1967) i: Bridges J.M. & Wiese W.L., Phys. Rev. A159, 31 (1967) k: Miller M.H., Wilkerson T.D., Roig R.A. & Bengston R.D., Phys. Rev. A9, 2312 (1974) --- lg3 Oscillator strength (log gf) from other work --- r_lg3 Reference to result lg3 number=2 a: Kurucz R.L. & Peytremann E., Smith. Astron. Obs. Spec. Report 362 (1975) b: Lambert D.L. & Warner B., MNRAS 138, 181 (1968) c: Biemont E. & Grevesse N., ADNDT 12, 217 (1973) d: Lambert D.L. & Luck R.E., MNRAS 183, 79 (1978) e: Aymar M., NIM 110, 211 (1973) f: Aymar M., Physica 66, 364 (1973) g: Wiese W. L. et al., (1969) h: Foster E.W., Proc. Phys. Soc. London 90, 275 (1967) i: Bridges J.M. & Wiese W.L., Phys. Rev. A159, 31 (1967) k: Miller M.H., Wilkerson T.D., Roig R.A. & Bengston R.D., Phys. Rev. A9, 2312 (1974) --- lg4 Oscillator strength (log gf) from other work --- r_lg4 Reference to result lg4 number=2 a: Kurucz R.L. & Peytremann E., Smith. Astron. Obs. Spec. Report 362 (1975) b: Lambert D.L. & Warner B., MNRAS 138, 181 (1968) c: Biemont E. & Grevesse N., ADNDT 12, 217 (1973) d: Lambert D.L. & Luck R.E., MNRAS 183, 79 (1978) e: Aymar M., NIM 110, 211 (1973) f: Aymar M., Physica 66, 364 (1973) g: Wiese W. L. et al., (1969) h: Foster E.W., Proc. Phys. Soc. London 90, 275 (1967) i: Bridges J.M. & Wiese W.L., Phys. Rev. A159, 31 (1967) k: Miller M.H., Wilkerson T.D., Roig R.A. & Bengston R.D., Phys. Rev. A9, 2312 (1974) --- lg5 Oscillator strength (log gf) from other work --- r_lg5 Reference to result lg5 number=2 a: Kurucz R.L. & Peytremann E., Smith. Astron. Obs. Spec. Report 362 (1975) b: Lambert D.L. & Warner B., MNRAS 138, 181 (1968) c: Biemont E. & Grevesse N., ADNDT 12, 217 (1973) d: Lambert D.L. & Luck R.E., MNRAS 183, 79 (1978) e: Aymar M., NIM 110, 211 (1973) f: Aymar M., Physica 66, 364 (1973) g: Wiese W. L. et al., (1969) h: Foster E.W., Proc. Phys. Soc. London 90, 275 (1967) i: Bridges J.M. & Wiese W.L., Phys. Rev. A159, 31 (1967) k: Miller M.H., Wilkerson T.D., Roig R.A. & Bengston R.D., Phys. Rev. A9, 2312 (1974) --- lg6 Oscillator strength (log gf) from other work --- r_lg6 Reference to result lg6 number=2 a: Kurucz R.L. & Peytremann E., Smith. Astron. Obs. Spec. Report 362 (1975) b: Lambert D.L. & Warner B., MNRAS 138, 181 (1968) c: Biemont E. & Grevesse N., ADNDT 12, 217 (1973) d: Lambert D.L. & Luck R.E., MNRAS 183, 79 (1978) e: Aymar M., NIM 110, 211 (1973) f: Aymar M., Physica 66, 364 (1973) g: Wiese W. L. et al., (1969) h: Foster E.W., Proc. Phys. Soc. London 90, 275 (1967) i: Bridges J.M. & Wiese W.L., Phys. Rev. A159, 31 (1967) k: Miller M.H., Wilkerson T.D., Roig R.A. & Bengston R.D., Phys. Rev. A9, 2312 (1974) --- S I lines and corresponding gf values Lambda(lab) Laboratory wavelength 0.1nm Transition Transition --- log(gf) HFR oscillator strength --- Wlambda Equivalent width 0.1pm Einf Einf eV A Abundance in the logarithmic scale calculated with the Holweger & Muller (1974) solar model --- u_A When :, the value was not retained in the final sample as explained in the text --- Patricia Bauer CDS 1993 Oct 20 J_A+AS_102_435.xml A new catalogue of H-alpha emission-line stars and small nebulae in the Small Magellanic Cloud J/A+AS/102/451 J/A+AS/102/451 Emission-line stars and PNe in the SMC A new catalogue of H-alpha emission-line stars and small nebulae in the Small Magellanic Cloud N Meyssonnier M Azzopardi Astron. Astrophys. Suppl. Ser. 102 451 1993 1993A&AS..102..451M H II regions Magellanic Clouds Stars, Be Stars, emission Planetary nebulae Surveys Magellanic Clouds stars: emission-line, Be HII regions planetary nebulae: general surveys catalogs An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.
H-alpha emission-line stars and small nebulae in SMC Note indicates that a note in file "notes" --- MA MA catalogue running number number=5 The acronym [MA93] is also found in the literature. The stars are numbered according to increasing right ascension. --- u_MA A colon (:) or a double colon (::) number=6 the colons following the number indicates that the Halpha emission-line nature of the object is doubtful or very doubtful, mainly due to its severe faintness or because it is a late-type star. --- Slit Availability of slit spectra number=1 other spectroscopic observations are marked: 's' subsequent medium resolution spectroscopic observations by us 'S' previous spectroscopic observations have been reported from: [1981MNRAS.194..613A] Aller, Keyes, Ross & O'Mara B.J. [1977A&AS...30..261A] Ardeberg & Maurice [1979A&A....75..120A] Azzopardi & Breysacher [1981A&A....95..191A] Azzopardi, Breysacher & Muratorio [1987MNRAS.227..161B] Barlow [1989ApJ...339..244M] Boroson & Liebert [1960MNRAS.121..337F] Feast, Thackeray & Wesselink [1990A&A...234..233H] Heydari-Malayeri [ever published?] Heydari-Malayeri & Leisy 1993, in preparation [1991ApJS...75..407M] Meatheringham & Dopita [1991ApJS...76.1085M] Meatheringham & Dopita [1988MNRAS.234..583M] Monk, Barlow & Clegg [1990ApJS...74...93R] Russell & Dopita [1976MNRAS.174..513W] Webster [1991A&AS...91..425W] Westerlund, Azzopardi, Breysacher & Rebeirot [1993A&AS..102..401V] Winckel van, Duerbeck & Schwarz [1986A&A...163..119Z] Zickgraf, Wolf, Stahl, Leitherer & Appenzeller [1989A&A...220..206Z] Zickgraf, Wolf, Stahl & Humphreys --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec Intens Rough estimate of Halpha intens. number=7 the relative intensity of the Halpha line is obtained from the measurement of the optical density (0 - 5) of the emission-line-peak on the digitized image of our 4-hour exposure objective-prism plate. --- Sp Three digits describing the spectrum number=2 The three digits describe the spectrum as it appears on our deepest objective-prism plate: (a) relative intensity of the continuum quoted from 1 (faint) to 5 (overexposed), "2-3" pointing out an optimum exposure; the additional symbol "T" denotes that a trace of continuum is barely visible above the sky background on our plate, while intensity "0" indicates that the related object does not show any continuous spectrum underlying the emission-lines, (b) relative strength of the Halpha emission-line estimated on a scale from 1 to 5, in which 1 represents a very weak line and 5 a very strong line, (c) estimate of the Halpha emission-line feature, where "1" denotes a sharp line, "2" a line appreciably widened and "3" a line which is diffuse to very diffuse. --- Object Nature or possible nature (:) of the objects number=3 Code for the nature of the objects: (1) H II region or filaments (2) supernova remnant (3) bubble or loop (4) compact or small HII region (5) PN or PN candidate (:) (6) VLE or VLE candidate (:) (7) Wolf-Rayet star (8) Peculiar Halpha emission-line stars with FeII and [FeII] emission --- Ident Cross-identifications and Cluster. number=4 The first word (followed by one or more blanks) contains cross-identifications separated by commas, in chronological order, given by a letter abbreviation followed by the number assigned by the respective authors who identified the object. Cluster information on the star location in connection with the SMC cluster system; a given star may lie either within a cluster or in its nearby surrounding field but that, of course, does not imply cluster membership. Abbreviations used in cross-identifications and Cluster designation: AB [1979A&A....75..120A] Azzopardi & Breysacher ARP [1959AJ.....64..254A] Arp AV [1982A&AS...50..291A] Azzopardi & Vigneau B [1976ORROE...1....1B] Bruck (Occas. Rep. R. Obs. Edinburgh No 1) DEM [1976MmRAS..81...89D] Davies, Elliot & Meaburn H [1986PASP...98.1113H] Hodge HW [1974AJ.....79..858H] Hodge & Wright J [1980ApJS...42....1J] Jacoby K [1956PASP...68..125K] Kron L [1961AJ.....66..169L] Lindsay; see note (*) Ln [1958MNRAS.118..172L] Lindsay MG [1985MNRAS.213..491M] Morgan & Good Mn [1992MNRAS.258..639M] Morgan Mo [1984MNRAS.209..241M] Morgan N [1955ApJS....2..315H] Henize NGC [see cat.<VII/1>] Dreyer 1888 (Mem.RAS XLIX) PMMR [1983A&AS...53..255P] Prevot, Martin, Maurice, Rebeirot & Rousseau R [1960MNRAS.121..337F] Feast, Thackeray & Wesselink RAW [1993A&AS...97..603R] Rebeirot, Azzopardi & Westerlund S [1955ApJS....2..315H] Henize (emission-line stars) Sa [1968AJ.....73..246S] Sanduleak Sk [1989AJ.....98..825S] Sanduleak SMP [1978PASP...90..621S] Sanduleak, McConnel & Philip SP [1981PASP...93..431S] Sanduleak & Pesch (*) Note that Lindsay (1961) did not provide finding charts for several emission objects listed in his catalogue, thus their identification is possible only with the help of their coordinates. When Lindsay's coordinates for an object do not match ours adequately, the Lindsay cross-identification "L" number is followed by a colon. Letter abbreviation for author who previously found the object: B Bruck 1976 (1976ORROE...1....1B) H Hodge 1986 (1986PASP...98.1113H) HW Hodge & Wright 1974 (1974AJ.....79..858H) K Kron 1956 (1956PASP...68..125K) Ln Lindsay 1958 (1961AJ.....66..169L) NGC Dreyer 1888 (cat. <VII/1>) --- Notes to table2 MA MA catalogue number --- Cont Increasing symbol indicating continuation --- Text Text of note; bibcodes are used for references --- Francois Ochsenbein CDS 1996 Sep 20 UNKNOWN UNKNOWN Original version Patricia Bauer [CDS] 12-Oct-1993 J_A+AS_102_451.xml Observational data for the kinematics of the local universe. II. Second set of radial velocity measurements. J/A+AS/102/57 J/A+AS/102/57 Observational data for the kinematics of the Observational data for the kinematics of the local universe. II. Second set of radial velocity measurements. L Bottinelli N Durand P Fouque R Garnier L Gouguenheim M Loulergue G Paturel C Petit P Teerikorpi Astron. Astrophys. Suppl. Ser. 102 57 1993 1993A&AS..102...57B catalogs galaxies: distances and redshifts radio lines: individual (21 cm) This paper is the second one in a series dedicated to the study of the kinematics of the local universe. It gives 361 new optical and radio redshifts measured at ESO, OHP and Nancay Observatories.
List of Vr PGC PGC number according to Paturel et al., A&AS 80, 299 (1989) --- Name Alternate name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec n_pos '*' means accurate position --- Vr Observed heliocentric radial velocity km/s u_Vr Uncertainty flag (:) --- e_Vr mean error on radial velocity in km/s km/s Site Site --- Notes Notes: + multiple measurement e elliptical galaxy & PGC28290=PGC28283 n Individual Notes (see below) --- Francois Ochsenbein CDS 1993 Apr 02 J_A+AS_102_57.xml The chemical evolution of the galactic disk II. Observational data. J/A+AS/102/603 J/A+AS/102/603 The chemical evolution of the galactic disk II The chemical evolution of the galactic disk II. Observational data. B Edvardsson J Andersen B Gustafsson D L Lambert P E Nissen J Tomkin Astron. Astrophys. Suppl. Ser. 102 603 1993 1993A&AS..102..603E stars: abundances *** No Description Available ***
Stellar equivalent widths for 16 stars observed both from ESO and McDonald (1) (first 43 spectral lines) Stellar equivalent widths ESO observations (NOTE 1%) Stellar equivalent widths McDonald observations Name Stellar identification (Catalogue+number) --- Obs Observed from ESO (E) or McDonald (M) --- OI__6158 Equivalent width for O I__6158.17 A 0.1pm OI__7771 Equivalent width for O I__7771.95 A 0.1pm OI__7774 Equivalent width for O I__7774.17 A 0.1pm OI__7775 Equivalent width for O I__7775.39 A 0.1pm NaI__6154 Equivalent width for Na I 6154.22 A 0.1pm NaI__6160 Equivalent width for Na I 6160.75 A 0.1pm MgI__8712 Equivalent width for Mg I 8712.69 A 0.1pm MgI__8717 Equivalent width for Mg I 8717.82 A 0.1pm AlI__8772 Equivalent width for Al I 8772.87 A 0.1pm AlI__8773 Equivalent width for Al I 8773.90 A 0.1pm SiI__6125 Equivalent width for Si I 6125.03 A 0.1pm SiI__6142 Equivalent width for Si I 6142.49 A 0.1pm SiI__6145 Equivalent width for Si I 6145.02 A 0.1pm SiI__6155 Equivalent width for Si I 6155.14 A 0.1pm SiI__7760 Equivalent width for Si I 7760.64 A 0.1pm SiI__7800 Equivalent width for Si I 7800.00 A 0.1pm SiI__8728 Equivalent width for Si I 8728.01 A 0.1pm SiI__8742 Equivalent width for Si I 8742.45 A 0.1pm CaI__5867 Equivalent width for Ca I 5867.57 A 0.1pm CaI__6161 Equivalent width for Ca I 6161.30 A 0.1pm CaI__6166 Equivalent width for Ca I 6166.44 A 0.1pm CaI__6169 Equivalent width for Ca I 6169.04 A 0.1pm TiI__5087 Equivalent width for Ti I 5087.06 A 0.1pm TiI__5113 Equivalent width for Ti I 5113.45 A 0.1pm TiI__5866 Equivalent width for Ti I 5866.46 A 0.1pm TiI__6126 Equivalent width for Ti I 6126.22 A 0.1pm FeI__5067 Equivalent width for Fe I 5067.16 A 0.1pm FeI__5083 Equivalent width for Fe I 5083.34 A 0.1pm FeI__5088 Equivalent width for Fe I 5088.16 A 0.1pm FeI__5090 Equivalent width for Fe I 5090.78 A 0.1pm FeI__5104 Equivalent width for Fe I 5104.44 A 0.1pm FeI__5109 Equivalent width for Fe I 5109.66 A 0.1pm FeI__5126 Equivalent width for Fe I 5126.20 A 0.1pm FeI__5127 Equivalent width for Fe I 5127.37 A 0.1pm FeI__5141 Equivalent width for Fe I 5141.75 A 0.1pm FeI__5809 Equivalent width for Fe I 5809.22 A 0.1pm FeI__5849 Equivalent width for Fe I 5849.69 A 0.1pm FeI__5852 Equivalent width for Fe I 5852.22 A 0.1pm FeI__5855 Equivalent width for Fe I 5855.08 A 0.1pm FeI__5856 Equivalent width for Fe I 5856.09 A 0.1pm FeI__5858 Equivalent width for Fe I 5858.78 A 0.1pm FeI__5859 Equivalent width for Fe I 5859.59 A 0.1pm FeI__5861 Equivalent width for Fe I 5861.11 A 0.1pm FeI__5862 Equivalent width for Fe I 5862.36 A 0.1pm FeI__6151 Equivalent width for Fe I 6151.62 A 0.1pm FeI__6157 Equivalent width for Fe I 6157.73 A 0.1pm FeI__6159 Equivalent width for Fe I 6159.38 A 0.1pm FeI__6165 Equivalent width for Fe I 6165.37 A 0.1pm FeI__6173 Equivalent width for Fe I 6173.34 A 0.1pm FeI__6187 Equivalent width for Fe I 6187.99 A 0.1pm FeI__6200 Equivalent width for Fe I 6200.32 A 0.1pm FeI__7745 Equivalent width for Fe I 7745.52 A 0.1pm FeI__7746 Equivalent width for Fe I 7746.60 A 0.1pm FeI__7751 Equivalent width for Fe I 7751.11 A 0.1pm FeI__7802 Equivalent width for Fe I 7802.51 A 0.1pm FeI__8713 Equivalent width for Fe I 8713.20 A 0.1pm FeI__8747 Equivalent width for Fe I 8747.44 A 0.1pm FeI__8757 Equivalent width for Fe I 8757.19 A 0.1pm FeII_5100 Equivalent width for Fe II 5100.66 A 0.1pm FeII_6149 Equivalent width for Fe II 6149.23 A 0.1pm NiI__5082 Equivalent width for Ni I 5082.35 A 0.1pm NiI__5084 Equivalent width for Ni I 5084.11 A 0.1pm NiI__5088 Equivalent width for Ni I 5088.54 A 0.1pm NiI__5088 Equivalent width for Ni I 5088.96 A 0.1pm NiI__5094 Equivalent width for Ni I 5094.42 A 0.1pm NiI__5099 Equivalent width for Ni I 5099.94 A 0.1pm NiI__5102 Equivalent width for Ni I 5102.97 A 0.1pm NiI__5115 Equivalent width for Ni I 5115.40 A 0.1pm NiI__5847 Equivalent width for Ni I 5847.00 A 0.1pm NiI__5857 Equivalent width for Ni I 5857.75 A 0.1pm NiI__6111 Equivalent width for Ni I 6111.08 A 0.1pm NiI__6130 Equivalent width for Ni I 6130.14 A 0.1pm NiI__6133 Equivalent width for Ni I 6133.98 A 0.1pm NiI__6175 Equivalent width for Ni I 6175.37 A 0.1pm NiI__6176 Equivalent width for Ni I 6176.82 A 0.1pm NiI__6177 Equivalent width for Ni I 6177.25 A 0.1pm NiI__6204 Equivalent width for Ni I 6204.61 A 0.1pm NiI__7748 Equivalent width for Ni I 7748.89 A 0.1pm NiI__7788 Equivalent width for Ni I 7788.93 A 0.1pm NiI__7797 Equivalent width for Ni I 7797.58 A 0.1pm YII_5087 Equivalent width for Y II 5087.43 A 0.1pm ZrII_5112 Equivalent width for Zr II 5112.27 A 0.1pm BaII_5853 Equivalent width for Ba II 5853.68 A 0.1pm BaII_6141 Equivalent width for Ba II 6141.73 A 0.1pm NdII_5089 Equivalent width for Nd II 5089.83 A 0.1pm NdII_5092 Equivalent width for Nd II 5092.80 A 0.1pm Stellar line-by-line chemical abundances for 16 stars observed both from ESO and McDonald Name Stellar identification (Catalogue+number) --- Obs Observed from ESO (E) or McDonald (M) --- A6158 =[ O/H] abundance rel. Sun O I 6158.17 A --- A7771 =[ O/H] abundance rel. Sun O I 7771.95 A --- A7774 =[ O/H] abundance rel. Sun O I 7774.17 A --- A7775 =[ O/H] abundance rel. Sun O I 7775.39 A --- A6154 =[Na/H] abundance rel. Sun Na I 6154.22 A --- A6160 =[Na/H] abundance rel. Sun Na I 6160.75 A --- A8712 =[Mg/H] abundance rel. Sun Mg I 8712.69 A --- A8717 =[Mg/H] abundance rel. Sun Mg I 8717.82 A --- A8772 =[Al/H] abundance rel. Sun Al I 8772.87 A --- A8773 =[Al/H] abundance rel. Sun Al I 8773.90 A --- A6125 =[Si/H] abundance rel. Sun Si I 6125.03 A --- A6142 =[Si/H] abundance rel. Sun Si I 6142.49 A --- A6145 =[Si/H] abundance rel. Sun Si I 6145.02 A --- A6155 =[Si/H] abundance rel. Sun Si I 6155.14 A --- A7760 =[Si/H] abundance rel. Sun Si I 7760.64 A --- A7800 =[Si/H] abundance rel. Sun Si I 7800.00 A --- A8728 =[Si/H] abundance rel. Sun Si I 8728.01 A --- A8742 =[Si/H] abundance rel. Sun Si I 8742.45 A --- A5867 =[Ca/H] abundance rel. Sun Ca I 5867.57 A --- A6161 =[Ca/H] abundance rel. Sun Ca I 6161.30 A --- A6166 =[Ca/H] abundance rel. Sun Ca I 6166.44 A --- A6169 =[Ca/H] abundance rel. Sun Ca I 6169.04 A --- A5087 =[Ti/H] abundance rel. Sun Ti I 5087.06 A --- A5113 =[Ti/H] abundance rel. Sun Ti I 5113.45 A --- A5866 =[Ti/H] abundance rel. Sun Ti I 5866.46 A --- A6126 =[Ti/H] abundance rel. Sun Ti I 6126.22 A --- A5067 =[Fe/H] abundance rel. Sun Fe I 5067.16 A --- A5083 =[Fe/H] abundance rel. Sun Fe I 5083.34 A --- A5088 =[Fe/H] abundance rel. Sun Fe I 5088.16 A --- A5090 =[Fe/H] abundance rel. Sun Fe I 5090.78 A --- A5104 =[Fe/H] abundance rel. Sun Fe I 5104.44 A --- A5109 =[Fe/H] abundance rel. Sun Fe I 5109.66 A --- A5126 =[Fe/H] abundance rel. Sun Fe I 5126.20 A --- A5127 =[Fe/H] abundance rel. Sun Fe I 5127.37 A --- A5141 =[Fe/H] abundance rel. Sun Fe I 5141.75 A --- A5809 =[Fe/H] abundance rel. Sun Fe I 5809.22 A --- A5849 =[Fe/H] abundance rel. Sun Fe I 5849.69 A --- A5852 =[Fe/H] abundance rel. Sun Fe I 5852.22 A --- A5855 =[Fe/H] abundance rel. Sun Fe I 5855.08 A --- A5856 =[Fe/H] abundance rel. Sun Fe I 5856.09 A --- A5858 =[Fe/H] abundance rel. Sun Fe I 5858.78 A --- A5859 =[Fe/H] abundance rel. Sun Fe I 5859.59 A --- A5861 =[Fe/H] abundance rel. Sun Fe I 5861.11 A --- A5862 =[Fe/H] abundance rel. Sun Fe I 5862.36 A --- A6151 =[Fe/H] abundance rel. Sun Fe I 6151.62 A --- A6157 =[Fe/H] abundance rel. Sun Fe I 6157.73 A --- A6159 =[Fe/H] abundance rel. Sun Fe I 6159.38 A --- A6165 =[Fe/H] abundance rel. Sun Fe I 6165.37 A --- A6173 =[Fe/H] abundance rel. Sun Fe I 6173.34 A --- A6187 =[Fe/H] abundance rel. Sun Fe I 6187.99 A --- A6200 =[Fe/H] abundance rel. Sun Fe I 6200.32 A --- A7745 =[Fe/H] abundance rel. Sun Fe I 7745.52 A --- A7746 =[Fe/H] abundance rel. Sun Fe I 7746.60 A --- A7751 =[Fe/H] abundance rel. Sun Fe I 7751.11 A --- A7802 =[Fe/H] abundance rel. Sun Fe I 7802.51 A --- A8713 =[Fe/H] abundance rel. Sun Fe I 8713.20 A --- A8747 =[Fe/H] abundance rel. Sun Fe I 8747.44 A --- A8757 =[Fe/H] abundance rel. Sun Fe I 8757.19 A --- A5100 =[Fe/H] abundance rel. Sun Fe II 5100.66 A --- A6149 =[Fe/H] abundance rel. Sun Fe II 6149.23 A --- A5082 =[Ni/H] abundance rel. Sun Ni I 5082.35 A --- A5084 =[Ni/H] abundance rel. Sun Ni I 5084.11 A --- A5088 =[Ni/H] abundance rel. Sun Ni I 5088.54 A --- A5088 =[Ni/H] abundance rel. Sun Ni I 5088.96 A --- A5094 =[Ni/H] abundance rel. Sun Ni I 5094.42 A --- A5099 =[Ni/H] abundance rel. Sun Ni I 5099.94 A --- A5102 =[Ni/H] abundance rel. Sun Ni I 5102.97 A --- A5115 =[Ni/H] abundance rel. Sun Ni I 5115.40 A --- A5847 =[Ni/H] abundance rel. Sun Ni I 5847.00 A --- A5857 =[Ni/H] abundance rel. Sun Ni I 5857.75 A --- A6111 =[Ni/H] abundance rel. Sun Ni I 6111.08 A --- A6130 =[Ni/H] abundance rel. Sun Ni I 6130.14 A --- A6133 =[Ni/H] abundance rel. Sun Ni I 6133.98 A --- A6175 =[Ni/H] abundance rel. Sun Ni I 6175.37 A --- A6176 =[Ni/H] abundance rel. Sun Ni I 6176.82 A --- A6177 =[Ni/H] abundance rel. Sun Ni I 6177.25 A --- A6204 =[Ni/H] abundance rel. Sun Ni I 6204.61 A --- A7748 =[Ni/H] abundance rel. Sun Ni I 7748.89 A --- A7788 =[Ni/H] abundance rel. Sun Ni I 7788.93 A --- A7797 =[Ni/H] abundance rel. Sun Ni I 7797.58 A --- A5087 =[ Y/H] abundance rel. Sun Y II 5087.43 A --- A5112 =[Zr/H] abundance rel. Sun Zr II 5112.27 A --- A5853 =[Ba/H] abundance rel. Sun Ba II 5853.68 A --- A6141 =[Ba/H] abundance rel. Sun Ba II 6141.73 A --- A5089 =[Nd/H] abundance rel. Sun Nd II 5089.83 A --- A5092 =[Nd/H] abundance rel. Sun Nd II 5092.80 A --- CDS 1993 May 28 J_A+AS_102_603.xml Stark widths of singly-ionized iron spectral lines J/A+AS/102/607 J/A+AS/102/607 Stark widths of singly-ionized iron spectral lines Stark widths of singly-ionized iron spectral lines J Puric S Djenize A Sreckovic S Bukvic S Pivalica J Labat Astron. Astrophys. Suppl. Ser. 102 607 1993 1993A&AS..102..607P atomic data line: profiles Strak broadening *** No Description Available ***
Singly-ionized iron spectral lines Stark widths Transition Designation of the transition --- N Note for transition: (1) for uv 1, (2) for uv 2 --- Lambda Wavelength nm T Temperature 10+4K N Electronic density 10+23.m-3 W Experimental Stark width 0.01nm Wp Predicted Stark width 0.01nm Patricia Bauer CDS 1993 Oct 12 J_A+AS_102_607.xml Millimeter continuum measurements of extragalactic radio sources. III. J/A+AS/102/611 J/A+AS/102/611 Millimeter continuum of extragal. sources III. Millimeter continuum measurements of extragalactic radio sources. III. H Steppe G Paubert A Sievers H P Reuter A Greve S Liechti B Le Floch W Brunswig C Menedez S Sanchez Astron. Astrophys. Suppl. Ser. 102 611 1993 1993A&AS..102..611S J/A+AS/122/271 : mm-monitoring of radio sources IV. (Reuter+ 1997) Active gal. nuclei BL Lac objects Galaxies, radio QSOs BL Lacertae objects: general galaxies: active quasars: general radio continuum: galaxies *** No Description Available ***
Catalog IAU IAU name --- Date Observing date "DD-MM-YY" HDJ Julian date at 0 h U.T. d o_S90 Number of independent observations (90 GHz) --- l_S90 limit flag on S90 --- S90 90 GHz (3.3 mm) flux density Jy e_S90 total error at 90 GHz number=2 The total error is the quadratic sum of a scatter error and a calibration error. The calibration error is 5% at 90 GHz and 10% at 150 and 230 GHz. Jy n_S90 See note number=1 An * denote that the rms uncertainty is 3 x rms A letter in the column 29 denote that the observation has been made at : a = 80 GHz b = 91 GHz c = 94 GHz d = 102 GHz e = 134 GHz f = 243 GHz --- o_S150 Number of independent observations (150 GHz) --- note1 An * denote a missing measurement --- S150 150 GHz (2 mm) flux density Jy e_S150 total error at 150 GHz number=2 The total error is the quadratic sum of a scatter error and a calibration error. The calibration error is 5% at 90 GHz and 10% at 150 and 230 GHz. Jy n_S150 See note number=1 An * denote that the rms uncertainty is 3 x rms A letter in the column 29 denote that the observation has been made at : a = 80 GHz b = 91 GHz c = 94 GHz d = 102 GHz e = 134 GHz f = 243 GHz --- o_S230 Number of independent observations (230 GHz) --- S230 230 GHz (1.3 mm) flux density Jy e_S230 total error at 230 GHz number=2 The total error is the quadratic sum of a scatter error and a calibration error. The calibration error is 5% at 90 GHz and 10% at 150 and 230 GHz. Jy n_S230 See note number=1 An * denote that the rms uncertainty is 3 x rms A letter in the column 29 denote that the observation has been made at : a = 80 GHz b = 91 GHz c = 94 GHz d = 102 GHz e = 134 GHz f = 243 GHz --- List of source titles IAU IAU source designation --- Name 3C or commonly used name --- Type QSO (quasar), BL Lac (BL Lac type object) GAL (galaxy) --- u_Type uncertainty flag on type --- l_z limit flag on redshift (z) --- z redshift --- u_z uncertainty flag on redshift --- Patricia Bauer CDS 1994 Feb 18 UNKNOWN UNKNOWN The electronic availability was delayed due to the death of the first author. A copy of Steppe's files was finally received from W. Brunswig in February 1994, and includes more observations than plotted on the Figures of the published paper. J_A+AS_102_611.xml Mesures d'etoiles doubles faite a Nice (4e serie) J/A+AS/102/643 J/A+AS/102/643 Mesure d'etoiles doubles Mesures d'etoiles doubles faite a Nice (4e serie) P Muller Astron. Astrophys. Suppl. Ser. 102 643 1993 1993A&AS..102..643M binaries: visual *** No Description Available ***
Double stars measurements Name ADS number or name --- Pos Position J2000.0 --- Date Date of observation yr angle Separation angle deg Note r = ronde, s = simple, P = Pas vu B --- l_dist limit flag on distance --- dist Distance arcsec n Number of observations --- Com Comments. A '*' starting character indicates individual notes (see below) --- Patricia Bauer CDS 1994 Oct 27 J_A+AS_102_643.xml Stroemgren four-colour uvby photometry of G5-type HD stars brighter than mv=8.6 J/A+AS/102/89 J/A+AS/102/89 Stroemgren four-colour uvby photometry of G5-type HD Stroemgren four-colour uvby photometry of G5-type HD stars brighter than mv=8.6 E H Olsen Astron. Astrophys. Suppl. Ser. 102 89 1993 1993A&AS..102...89O catalogs Galaxy: evolution solar neighborhood stars: fundamental parameters stars: late-type techniques: photometric *** No Description Available ***
121 uvby standards, S cat, standard system (Southern SAT survey) 84 uvby standards, L cat, standard system (Northern KPNO survey) 43 uvby standards, N cat, standard system (Northern SPM survey) HR HR=BS (Bright Star Catalogue) number --- V transformed to the standard Johnson V mag. mag e_V mean error on V mag b-y b-y mag e_(b-y) mean error on (b-y) mag m1 = (v-b) - (b-y) mag e_(m1) mean error on m1 mag c1 = (u-v) - (v-b) mag e_(c1) mean error on c1 mag w_V weight of V --- w_col weight of 4-colour indices --- NN Number of nights --- D(V) Difference V(standard) - V(transformed) mag D(b-y) Difference (b-y)(st) - (b-y)(tr) mag D(m1) Difference m1(st) - m1(tr) mag D(c1) Difference c1(st) - c1(tr) mag The catalogue HD ? HD (Henry Draper) designation --- Mult Identification of visual double star components included in the diaphragm --- Prog Program star list G = G-type star (see paper, section 2.1.1) C = Calibration star (see paper, section 2.1.2) H = Backup program (see paper, section 2.1.3) L = Luyten NGP star Y = Hyades star O = Coma star * = miscellaneous reasons --- DM Durchmusterung identification (BD, CD or CP in bytes 17-18; SZZNNNNN on bytes 19-26; appended letter in byte 27 NB! This column may be blank or contain alternative identification --- Other Alternative identification --- T Transformation used (see paper) D = GKV transformation, G or C = GKIII transformation, % W or blank = BAF transformation --- V transformed to the standard Johnson V mag. mag e_V mean error on V mag b-y on standard Crawford-Barnes system mag e_(b-y) mean error on (b-y) mag m1 on standard Crawford-Barnes system mag e_(m1) mean error on m1 mag c1 on standard Crawford-Barnes system mag e_(c1) mean error on c1 mag w_V weight of V --- w_col weight of 4-colour indices --- NN Number of nights --- Note N = visual double star not listed in IDS S = star selected as a potential secondary uvby standard * = individual note (see paper) --- Francois Ochsenbein CDS 1994 Jun 25 UNKNOWN UNKNOWN *27-Nov-1993: First archived; table18 had 254 non-blank erroneous HD numbers. *25-Jun-1994: Removed in table18 the erroneous HD numbers. J_A+AS_102_89.xml Collected photometry of FK Comae Berenices J/A+AS/103/183 J/A+AS/103/183 Collected photometry of FK Comae Berenices Collected photometry of FK Comae Berenices L Jetsu I Tuominen A Antov B W Bopp P F Chugainov K N Grankin S Linnaluoto S Yu Melnikov H L Nations K P Panov V S Shevchenko Astron. Astrophys. Suppl. Ser. 103 183 1994 1994A&AS..103..183J stars: individual (FK Com) stars: variables: general New photometric observations of FK Comae Berenices are combined to the previously published photometry and a firm basis established for the long--term phometric studies of this rapidly rotating late--type giant. The methods used to combine a quarter of a century of observations into a homogeneous set of standard Johnson UBVRI photometry are presented.
Johnson UBVRI photometry SET Subset number --- HJD Heliocentric Julian day d U U magnitude, value 0.000 means no observation mag B B magnitude, value 0.000 means no observation mag V V magnitude, value 0.000 means no observation mag R R magnitude, value 0.000 means no observation mag I I magnitude, value 0.000 means no observation mag F Flare detection : F=1=normal flare F=2=flare (detected with U-band) F=2=flare? (detected without U-band) --- Patricia Bauer CDS 1993 Oct 28 J_A+AS_103_183.xml Multicolor Photometry of Clusters of Galaxies: A3284, A3305 and A1942 J/A+AS/103/245 J/A+AS/103/245 Multicolor Photometry of Clusters of Galaxies Multicolor Photometry of Clusters of Galaxies: A3284, A3305 and A1942 E Molinari M Banzi A Buzzoni G Chincarini M D Pedrana Astron. Astrophys. Suppl. Ser. 103 245 1994 1994A&AS..103..245M galaxies: clusters: general galaxies: evolution galaxies: photometry We present complete multicolor photometry in the Gunn system for the three clusters of galaxies A3284, A3305 and A1942 at redshift z~0.2. INVENTORY magnitudes and colours have been obtained for over 1,000 objects in the three fields down to g=24, and with a good completeness level in the detections (85% or better) about one magnitude brighter. By fitting with King profiles the r counts we derived the total number of galaxies and the core radius down to the r magnitude limit in each cluster. These are N_TOT_=146 galaxies and R_c_=0.24 Mpc for A3284, N_TOT_=129 and R_c_=0.20 Mpc for A3305, N_TOT_=130 and R_c_=0.24 Mpc for A1942. The observed mean redshift of the clusters is z=0.150+/-0.001 for A3284, z=0.157+/-0.001 for A3305, and z=0.226+/-0.001 for A1942. The c-m diagrams and the g-i colour distribution as well as the two-colour diagrams are used to single out early-type galaxies and spirals on the basis of their different photometric properties. This approach aimed at a self-consistent classification of galaxies on the basis of photometric indicators will be further developed for a systematic study of the galaxy population in distant clusters.
Photometric catalog of A3284 Photometric catalog of A3305 Photometric catalog of A1942 CN Catalog number --- x x coordinate of the object pix y y coordinate of the object pix g g magnitude (Gunn system) mag r r magnitude (Gunn system) mag i i magnitude (Gunn system) mag g-r g-r color mag g-i g-i color mag Riso isophotal radius in the r magnitude pix Patricia Bauer CDS 1993 Oct 25 J_A+AS_103_245.xml Atomic Data from the IRON Project. II. Effective collision strengths for infrared transitions in carbon-like ions J/A+AS/103/273 J/A+AS/103/273 IRON Project II. C-like ions Atomic Data from the IRON Project. II. Effective collision strengths for infrared transitions in carbon-like ions D J Lennon V M Burke Astron. Astrophys. Suppl. Ser. 103 273 1994 1994A&AS..103..273L J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. FeII collision strengths J/A+A/293/967 : IRON Project VII. FeII radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project. XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data We present new calculations of cross-sections for the electron impact excitation of carbon-like ions from N II to S XI, paying particular attention to the infrared transitions between the 2p^2^ ^3^P J=0,1,2 ground state fine-structure levels. We also give rate coefficients, assuming a Maxwellian electron velocity distribution, in the form of effective collision strengths for these transitions up to an electron temperature of 10^5^ K. We also give results for transitions involving the other 2p^2^ terms (^1^D and ^1^S) as well as the 2s2p^3^ (^5^S) term. The present results are in excellent agreement with a number of similar calulations available in the literature but are more comprehensive in scope.
Effective collision strengths for N II transition Effective collision strengths for O III transition Effective collision strengths for F IV transition Effective collision strengths for Ne V transition Effective collision strengths for Na VI transition Effective collision strengths for Mg VII transition Effective collision strengths for Al VIII transition Effective collision strengths for Si IX transition Effective collision strengths for P X transition Effective collision strengths for S XI transition logT Temperature K 3P0-3P1 Effective collision strength --- 3P0-3P2 Effective collision strength --- 3P1-3P2 Effective collision strength --- 3P-1D2 Effective collision strength --- 3P-1S0 Effective collision strength --- 3P-5S2 Effective collision strength --- 1D2-1S0 Effective collision strength --- Francois Ochsenbein CDS 1993 Oct 07 J_A+AS_103_273.xml Spectral lines unaffected by instrumental polarization. II. Selected lines of astrophysical interest. J/A+AS/103/293 J/A+AS/103/293 Spectral lines unaffected by instrumental polarizati Spectral lines unaffected by instrumental polarization. II. Selected lines of astrophysical interest. E Vela Villahoz J Sanchez Almeida A D Wittmann Astron. Astrophys. Suppl. Ser. 103 293 1994 1994A&AS..103..293V instrumental polarization magnetic field measurements Zeeman efect Lines with no linear polarization induced by Zeeman effect are unaffected by instrumental polarization. We compile 86 such electric dipole lines with differing temperature and magnetic field sensitivities. In addition, we list 420 spectral lines which produce negligible linear polarization. In most cases, this second set can also be regarded as lines unaffected by instrumental polarization.
Lines with no linear polarization S Species --- lambda Wavelength (Angstroems) 0.1nm Trans Transition --- geff Effective Lande factor --- W Equivalent width (milli-Angstroems) 0.1pm Blend Blends --- Lines with negligible linear polarization S Species --- lambda Wavelength (Angstroems) 0.1nm Trans Transition --- geff Effective Lande factor --- R Ratio linear to circular polarization % W Equivalent width (milli-Angstroems) 0.1pm Blend Blends ---- Francois Ochsenbein CDS 1993 Sep 20 J_A+AS_103_293.xml The Second Quito Astrolabe Catalogue J/A+AS/103/427 J/A+AS/103/427 The Second Quito Astrolabe Catalogue The Second Quito Astrolabe Catalogue Y B Kolesnik H Davila Astron. Astrophys. Suppl. Ser. 103 427 1994 1994A&AS..103..427K astrometry catalogs reference systems The paper contains 515 individual corrections {DELTA}{alpha} and 235 corrections {DELTA}{delta} to FK5 and FK5Supp. stars and 50 corrections to their proper motions computed from observations made with the classical Danjon astrolabe OPL-13 at Quito Astronomical Observatory of Ecuador National Polytechnical School during a period from 1964 to 1983. These corrections cover the declination zone from -30deg to +30deg. Mean probable errors of catalogue positions are 0.047" in {alpha}cos{delta} and 0.054" in {delta}. The systematic trends of the catalogue {DELTA}{alpha}_{alpha}_cos {delta},{DELTA}{alpha}_{delta}_cos{delta}, {DELTA}{delta}_{alpha}_, {DELTA} {delta}_{delta}_ are presented for the observed zone.
The Second Quito Astrolabe Catalogue FK5 FK5 or FK5 Supp. number of a star --- N Designation of the star's subset. --- V Visual magnitude mag Sp Spectral type --- MEp Mean epoch of the observation from 1900 yr RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s cRA Correction to the adopted right ascension at the mean epoch of observation s e_cRA Probable error of the right ascension correction s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec cDE Correction to the adopted declination at the mean epoch of observation arcsec e_cDE Probable error of the declination correction arcsec Corrections to FK5 proper motions in right ascension and declination FK5 FK5 or FK5 supp. number of star --- N Designation of the star's subset. number=1 Letter F denotes that star is contained in FK5 or FK5 Extension list. Letter S denotes that star is contained only in FK5 Supp.list --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s cmuRA Correction to proper motion in right ascension s e_cmuRA Probable error on the correction to proper motion in right ascension s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec cmuDE Correction to proper motion in declination arcsec e_cmuDE probable error on the correction to proper motion in declination arcsec Patricia Bauer CDS 1994 Mar 01 J_A+AS_103_427.xml High-resolution optical spectroscopy of the hot R CrB star V348 Sgr J/A+AS/103/445 J/A+AS/103/445 High-resolution optical spectroscopy of the High-resolution optical spectroscopy of the hot R CrB star V348 Sgr U Leuenhagen U Heber C S Jeffery Astron. Astrophys. Suppl. Ser. 103 445 1994 1994A&AS..103..445L line: identification stars: atmospheres stars: chemically peculiar stars: emission-line, Be stars: individual (V348 Sgr) supergiants High resolution optical spectra of the unique hot R CrB star V348 Sgr are presented and more than 500 spectral lines of 14 elements are identified. The spectrum is very complex and four types of line profiles can be distinguished: a) pure absorption lines, b) P-Cygni lines, c) pure emission lines and d) P-Cygni (HeI) or emission (CII) profiles with central absorption reversal. The spectrum is interpreted as that of an expanding atmosphere of small optical thickness with wind velocities between 150 and 200 km/s. Hydrogen is definitely present in the expanding atmosphere. The absorption line spectrum is very similar to that of the extreme helium stars DY Cen and LSE 78.
Identified lines of the present spectra Name Element designation --- MN Multiplet number --- n_MN An * correspond to none, an F correspond to the multiplet number (1. F = 1F) --- LC Line class number=1 a: pure absorption b: blue-shifted absorption and red-shifted emission (P-Cygni profil) b/c: emission line with uncertain blue absorption c: pure emission d: central reversal in emission components of lines of Class b+c --- u_LC uncertainty flag on line class --- W Laboratory wavelength 0.1nm T Transition --- R Comments --- Patricia Bauer CDS 1994 Mar 02 J_A+AS_103_445.xml The Arcetri Catalogue of H2O Maser Sources Update J/A+AS/103/541 J/A+AS/103/541 The Arcetri Catalogue of H2O Maser Sources Update The Arcetri Catalogue of H2O Maser Sources Update J Brand R Cesaroni P Caselli M Catarzi C Codella G Comoretto G P Curioni P Curioni S Di Franco M Felli C Giovanardi L Olmi F Palagi F Palla D Panella G Pareschi E Rossi N Speroni G Tofani Astron. Astrophys. Suppl. Ser. 103 541 1994 1994A&AS..103..541B catalogs radio lines: ISM radio lines: stars An update is presented of the Arcetri Atlas of water masers (Comoretto et al. 1990). It contains the results of observations of water masers with the Medicina 32-m antenna. The observed sources were all discovered in the period 1989-1993, and were found either directly in the course of our own programs or were taken from the literature in which case they were re-observed at Medicina. We give the observed parameters of 214 sources in tabular form, and present all the spectra of the 141 detections.
Parameters of H2O observations of 214 sources IRAS IRAS name --- Name Other name(s) --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Clas Class --- Date Date of observation --- res Spectral resolution km/s Scan Scan number --- Sig 1 sigma rms noise in spectrum Jy Vmin minimum velocity of the emission (Note 1) km/s Vmax maximum velocity of the emission (Note 1) km/s Vpeak Velocity of peak signal (Note 2) km/s n_Vpeak (Note 2) --- Fp Peak flux Jy Stot Integrated flux Jy.km/s R Reference codes (Note 3) --- Patricia Bauer CDS 1993 Nov 03 Jan Brand J_A+AS_103_541.xml UBVRI photoelectric photometry of bright southern early-type galaxies J/A+AS/103/573 J/A+AS/103/573 UBVRI photoelectric photometry of bright southern UBVRI photoelectric photometry of bright southern early-type galaxies P Poulain J -L Nieto Astron. Astrophys. Suppl. Ser. 103 573 1994 1994A&AS..103..573P galaxies: elliptical and lenticular, cD galaxies: photometry UBVRI multi-aperture photometry of 207 bright southern galaxies and of 72 objects of an additional list is presented. These observations were made for obtaining the magnitude scale zero-point as an accurate determination of the sky background for a two-dimensional photometry program concerning these galaxies. We have also inferred the asymptotic magnitudes, color indices and effective apertures of these objects. Our results are in good agreement with those of others authors.
Multiaperture photometry of key-program galaxies Multiaperture photometry of additional galaxies Name NGC or IC or "Anonymous" name --- ESO ESO number --- Type Revised Morphological type T --- log(A) Aperture 0.1arcsec V V magnitude mag U-B U-B colour mag B-V B-V colour mag V-R V-R colour mag V-I V-I colour mag N Number of observations --- R Notes (* = subtracted star) --- Asymptotic magnitudes, mean color indices and effective radii for key-program galaxies Asymptotic magnitudes, mean color indices and effective radii for additional galaxies Name NGC or IC or "Anonymous" name --- ESO ESO number --- Type Revised Morphological type T --- Bt Asymtotic magnitude Bt mag (U-B)e Mean color index (U-B)e mag (B-V)e Mean color index (B-V)e mag (V-R)e Mean color index (V-R)e mag (V-I)e Mean color index (V-I)e mag log(Ae) Effective aperture 0.1arcsec R Notes: 1: Already published in A&AS 72,215 (1988) 2: August 1986 unpublished values 3: Values deduced from other sources --- Bibliography of key-program galaxies Name NGC or IC or "Anonymous" name --- ESO ESO/Uppsala name of the galaxy --- Bands Bands available for the galaxy --- R References (See Table 4) --- References of photoelectric photometry of key-program galaxies R1 Reference number of table 3 --- R2 References --- Bands Bands available for the galaxy --- Patricia Bauer CDS 1993 Oct 29 J_A+AS_103_573.xml Spectral coefficients of emission and absorption due to ion-atom radiation collisions in solar atmosphere J/A+AS/103/57 J/A+AS/103/57 Spectral coefficients of emission and absorption Spectral coefficients of emission and absorption due to ion-atom radiation collisions in solar atmosphere A A Mihajlov M S Dimitrijevic L J M Ignjatovic Z Djuric Astron. Astrophys. Suppl. Ser. 103 57 1994 1994A&AS..103...57M atomic data atomic processes radiation mechanisms: thermal Sun: atmosphere Spectral coefficients of spontaneous emission and absorption (for 365nm <= {lambda} <= 820nm range) due to ion-atom radiation processes H^+^ + H(1s) <--> H^+^_2_(1{SIGMA}_g_) and H^+^ + H(1s) <--> H(1s) +H^+^ are presented. Calculations have been performed within semiclassical approach for standard solar photosphere and chromosphere models. The presented numerical results enable the inclusion of considered ion-atom radiative processes in the optical depth calculation for the layers mentioned. These results might be of interest as well for other astrophysical plasmas with dominant hydrogen component and temperatures around 6000 K.
Basic plasma parameters for solar photospheric model of Maltby et al. (1986), as a function of height. Basic plasma parameters for solar chromospheric model of Vernazza et al. (1981) (model C) h Height km T Plasma temperature K Ne Electron density cm-3 Nth Total hydrogen density cm-3 eta_e1 (N(H+)/NE)*(N(H)/Ni) ratio number=1 N(H+) is the proton density, Ni is the total density of positive atomic ions and N(H) is the atom (H(1s)) density --- eta_ea N(H+)/Ne ratio number=1 N(H+) is the proton density, Ni is the total density of positive atomic ions and N(H) is the atom (H(1s)) density --- Emissivity as a function of wavelength and height for solar photospheric model of Maltby et al. (1986). Emissivity as a function of wavelength and height for solar chromospheric model of Vernazza et al. (1981) h Height km e365 Emissivity at 365 nm W/cm3/nm e400 Emissivity at 400 nm W/cm3/nm e500 Emissivity at 500 nm W/cm3/nm e600 Emissivity at 600 nm W/cm3/nm e700 Emissivity at 700 nm W/cm3/nm e820 Emissivity at 820 nm W/cm3/nm Spectral absorption coefficient as a function of wavelength and height for solar photospheric model of Maltby et al. (1986). Spectral absorption coefficient as a function of wavelength and height for solar chromospheric model of Vernazza et al. (1981) h Height km K365 Spectral absorption coefficient at 365 nm cm-1 K400 Spectral absorption coefficient at 400 nm cm-1 K500 Spectral absorption coefficient at 500 nm cm-1 K600 Spectral absorption coefficient at 600 nm cm-1 K700 Spectral absorption coefficient at 700 nm cm-1 K820 Spectral absorption coefficient at 820 nm cm-1 Francois Ochsenbein CDS 1993 Nov 17 J_A+AS_103_57.xml Evolutionary sequences for massive close binary stars with Magellanic Cloud metallicities with Rogers-Iglesias opacities J/A+AS/103/67 J/A+AS/103/67 Evolutionary sequences for massive close binary Evolutionary sequences for massive close binary stars with Magellanic Cloud metallicities with Rogers-Iglesias opacities C De Loore D Vanbeveren Astron. Astrophys. Suppl. Ser. 103 67 1994 1994A&AS..103...67D binaries: close Magellanic Clouds stars: evolution stars: Wolf-Rayet Tables of evolutionary sequences for massive stars with metallicities Z=0.002 and Z=0.01 in the mass range 9 to 40 M_{sun}_ and mass ratios 0.9 and 0.6 are presented. The orbital periods are chosen such that mass transfer according to case B occurs, i.e. mass exchange after core hydrogen exhaustion, during semi-detached and contact phases. The evolutionary code used by de Loore & De Greve (1992) for galactic massive close binaries was updated, i.e. new thermodynamic quantities and new opacities were installed. The evolution of both components is followed simultaneously. Stellar wind mass loss rates during the OB phase are scaled according to the radiatively driven wind theory. Wolf-Rayet mass loss rates are assumed to be independent of metallicity. The models presented here may be used to interpret and evaluate the observations of Wolf-Rayet stars and massive binary X-ray sources in the Small and Large Magellanic Clouds.
LMC abundances (Table3 to Table15) SMC abundances (Table16 to Table29) IM1 Initial mass of the primary Sun IM2 Initial mass of the secondary Sun Phase See note number=1 The different phases is as follows: ZAMS: Zero Age Main Sequence RP1: Red Point of the primary component Xc1=0: end of core hydrogen burning of the primary RLOFi: onset of a case B of Roche Lobe Overflow Lmin: minimum luminosity of the primary Xat<0.76 (SMC, or 0.74 (LMC): hydrogen abundance of the primary drops below its initial value CHeB1i: onset of core helium burning of the primary VHeB1i: onset of core helium burning of the primary RLOFf: end of Roche Lobe Overflow Yc1=0:end of core helium burning of the primary RP2: red point of the secondary Xc2=0: end core hydrogen burning of the secondary. Teffmin2: minimum of the effective temperature of the secondary Teffmax2: maximum of the effective temperature of the secondary WNL1,WNE1, WC1 denote the onset of the different Wolf-Rayet phases, the WNL,WNE and WC-phases of the primary. --- Age Age yr M1 Mass of the primary Sun ML1 Mass loss rate of the primary Sun/yr lofTeff1 Effective temperature of the primary --- logL1 Luminosity of the primary --- XC1 Central hydrogen content of the primary --- YC1 Central helium content of the primary --- XAT1 Surface hydrogen abundance of the primary --- Rad1 Radius of the primary Sun MCC1 Convective core mass of the primary Sun Period Period d M2 Mass of the secondary Sun ML2 Mass loss rate of the secondary Sun/yr lofTeff2 Effective temperature of the secondary --- logL2 Luminosity of the secondary --- XC2 Central hydrogen content of the secondary --- YC2 Central helium content of the secondary --- XAT2 Surface hydrogen content of the secondary --- Rad2 Radius of the secondary Sun MCC2 Convective core mass of the secondary Sun James Marcout CDS 1993 Sep 09 J_A+AS_103_67.xml Line identifications in a fireball spectrum J/A+AS/103/83 J/A+AS/103/83 Line identifications in a fireball spectrum Line identifications in a fireball spectrum J Borovicka Astron. Astrophys. Suppl. Ser. 103 83 1994 1994A&AS..103...83B line: identification meteors: spectra 305 emission lines were found in a spectrum of a fireball of -9th magnitude. The identification of most of the lines is given. Also a detailed tracing of the spectrum in the range 3600 - 6600 A is presented. The tracing contains also computed synthetic spectrum and both spectra can be easily compared. The following species were found in the spectrum: Fe I, Na I, Mg I, Al I, Ca I, Ti I, Cr I, Mn I, Ni I, Mg II, Si II, Ca II, Fe II, FeO, probably also Si I, Ba II, C_2_, and possibly V I, Co I, Cu I, Ti II. The presence of other chemical elements in meteor spectra is discussed.
Identifications of spectral lines observed in the spectrum of the bright meteor EN 151068 No Line number number= One observed line may be formed by several lines. 1) contribution of Fe II 4583.85 A ? 2) possible contribution of C III - 1 3) contribution of C_2 4) only fragment? 5) cannot explain the whole line 6) overexposed line p.: point (boundaries of meteor points used are marked) 2nd: 2nd second spectrum --- Lambda_obs Observed wavelength number= One observed line may be formed by several lines. 1) contribution of Fe II 4583.85 A ? 2) possible contribution of C III - 1 3) contribution of C_2 4) only fragment? 5) cannot explain the whole line 6) overexposed line p.: point (boundaries of meteor points used are marked) 2nd: 2nd second spectrum 0.1nm Lambda Laboratory wavelength number= One observed line may be formed by several lines. 1) contribution of Fe II 4583.85 A ? 2) possible contribution of C III - 1 3) contribution of C_2 4) only fragment? 5) cannot explain the whole line 6) overexposed line p.: point (boundaries of meteor points used are marked) 2nd: 2nd second spectrum 0.1nm Atom Identification: atom and multiplet or molecule and vibrational band or "?" for an unidentified line number= One observed line may be formed by several lines. 1) contribution of Fe II 4583.85 A ? 2) possible contribution of C III - 1 3) contribution of C_2 4) only fragment? 5) cannot explain the whole line 6) overexposed line p.: point (boundaries of meteor points used are marked) 2nd: 2nd second spectrum --- E_1 lower excitation potential number= One observed line may be formed by several lines. 1) contribution of Fe II 4583.85 A ? 2) possible contribution of C III - 1 3) contribution of C_2 4) only fragment? 5) cannot explain the whole line 6) overexposed line p.: point (boundaries of meteor points used are marked) 2nd: 2nd second spectrum eV log(gf) (oscillator strength) number= One observed line may be formed by several lines. 1) contribution of Fe II 4583.85 A ? 2) possible contribution of C III - 1 3) contribution of C_2 4) only fragment? 5) cannot explain the whole line 6) overexposed line p.: point (boundaries of meteor points used are marked) 2nd: 2nd second spectrum --- I_com computed line intensity number= One observed line may be formed by several lines. 1) contribution of Fe II 4583.85 A ? 2) possible contribution of C III - 1 3) contribution of C_2 4) only fragment? 5) cannot explain the whole line 6) overexposed line p.: point (boundaries of meteor points used are marked) 2nd: 2nd second spectrum 100W/sr Rem remark --- Observed calibrated spectrum in the range 3575-4080 A at the meteor point 15F (2nd order) Observed calibrated spectrum in the range 4050-4420 A at the meteor point 19F (2nd order) Observed calibrated spectrum in the range 4400-6600 A at the meteor point 13F (1st order) Lambda Wavelength (valid for the main piece) number= The point 13F is the brightest meteor point. The short wavelengths were, however, better observable in the second order spectra at different meteor points and these spectra were used for line identifications. The spectra at different points cannot be simply joined, because the meteor brightness and physical conditions were different at different points. The data given in the three files spec-* were used for drawing the solid line in Fig.4 of the paper. 0.1nm OIR Observed intensity of radiation (including the radiation of the fragments) in 10+9erg/s/A/sr number= The point 13F is the brightest meteor point. The short wavelengths were, however, better observable in the second order spectra at different meteor points and these spectra were used for line identifications. The spectra at different points cannot be simply joined, because the meteor brightness and physical conditions were different at different points. The data given in the three files spec-* were used for drawing the solid line in Fig.4 of the paper. kW/nm/sr Patricia Bauer CDS 1994 Jan 13 J_A+AS_103_83.xml Grids of massive stars with high mass loss rates. V. From 12 to 120 Mo at Z=0.001, 0.004, 0.008, 0.020 and 0.040 J/A+AS/103/97 J/A+AS/103/97 Grids of massive stars with high mass loss rates. V Grids of massive stars with high mass loss rates. V. From 12 to 120 Mo at Z=0.001, 0.004, 0.008, 0.020 and 0.040 G Meynet A Maeder G Schaller D Schaerer C Charbonnel Astron. Astrophys. Suppl. Ser. 103 97 1994 1994A&AS..103...97M Hertzsprung-Russell (HR diagram) stars: evolution stars: interiors stars: mass-loss Most outputs of massive star evolution critically depend on the mass loss rates. In order to broaden the comparison basis and to illustrate the effects of different mass loss rates, we have computed new sets of models, with initial masses between 12 and 120 M_{sun}_, and metallicities, Z, between 0.001 and 0.040, with a mass loss rate increased by a factor of two during the phases when the stellar winds are believed to be essentially driven by the radiation pressure. A moderate core-overshooting and the new radiative opacities from Iglesias et al. (1992) and Kurucz (1991) were taken into account. These models complete the homogeneous and extended theoretical database formed by the previous grids of this series, computed by Schaller et al. (1992) for Z=0.020 and Z=0.001, by Schaerer et al. (1992, 1993) for Z=0.008 and Z=0.040 and by Charbonnel et al. (1993) for Z=0.004. This paper closes this series. Of particular interest is the predicted behaviour of metal rich stars such as may be found in the inner regions of our Galaxy. New evolutionary connexions are found, in particular we show that the most massive and metal rich stars may spend a relatively long time as He and N enriched stars and may even end their evolution as white dwarfs.
120 M , z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 20 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 15 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 12 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 120M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 20 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 15 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 120 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 20 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 15 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 120 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 20 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 120 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases NB number of selected point --- Age age yr Mass actual mass in solar masses Sun logL log(luminosity) in solar units Sun logTe log(effective temperature) K X H surface abundance (mass fraction) --- Y He surface abundance (mass fraction) --- C12 12C surface abundance (mass fraction) --- C13 13C surface abundance (mass fraction) --- N14 14N surface abundance (mass fraction) --- O16 16O surface abundance (mass fraction) --- O17 17O surface abundance (mass fraction) --- O18 18O surface abundance (mass fraction) --- Ne20 20Ne surface abundance (mass fraction) --- Ne22 22Ne surface abundance (mass fraction) --- QCC core mass fraction --- logTu log(uncorrected Teff) (WR stars only) K logMdot log(mass loss rate) Sun/yr log(rho_c) log(central density) g/cm3 logTc log(central temperature) K Xc H central abundance (mass fraction) --- Yc He central abundance (mass fraction) --- C12c 12C central abundance (mass fraction) --- C13c 13C central abundance (mass fraction) --- N14c 14N central abundance (mass fraction) --- O16c 16O central abundance (mass fraction) --- O17c 17O central abundance (mass fraction) --- O18c 18O central abundance (mass fraction) --- Ne20c 20Ne central abundance (mass fraction) --- Ne22c 22Ne central abundance (mass fraction) --- Patricia Bauer CDS 1993 Sep 29 J_A+AS_103_97.xml Proper motion study of the globular cluster M 3 J/A+AS/104/161 J/A+AS/104/161 Proper motion study of the globular cluster M3 Proper motion study of the globular cluster M 3 H -J Tucholke R -D Scholz P Brosche Astron. Astrophys. Suppl. Ser. 104 161 1994 1994A&AS..104..161T astrometry galaxies: clusters: individual (M 3) reference systems We present proper motions for stars in the field of the galactic globular cluster NGC 5272 (M 3). This study forms part of the Bonn programme of globular cluster proper motions. 14 plates were taken with the Bonn double refractor, spanning epoch differences of up to 85 years. Relative proper motions for all well-measurable stars in the 1.5deg x 1.5deg field covered by the plates were derived. Typical proper motion errors are 0.5-1.2 milliarcsec/year. The cluster membership of UV-bright and variable stars is discussed. The proper motions are compared with the accurate relative proper motions of Cudworth (1979) and with the absolute proper motions from Schmidt plates referred to galaxies of Scholz et al. (1993). The latter comparison enables us to tie the proper motions of the stars and the mean proper motion of M 3 to an inertial system. The absolute proper motions of Hipparcos stars in the field will be useful for an extragalactic calibration of the Hipparcos proper motion system.
Data for the stars in the field of M 3 Name vZ designation (von Zeipel, 1908) --- u_Name uncertain identifier flag --- RAh Right ascension J2000.0 (epoch 1950.0) h DEd Declination J2000.0 (epoch 1950.0) deg pmRA absolute proper motion in right ascension mas/a e_pmRA internal error in proper motion alpha mas/a pmDE absolute proper motion in delta mas/a e_pmDE internal error in proper motion delta mas/a Prob membership probability % Npos Number of positions form which the proper motion was derived --- B B magnitude mag K K designation (Kuestner, 1922) --- u_K uncertain identifier flag --- San San designation (Sandage 1953- Series I; 1970) --- u_San uncertain identifier flag --- SK SK designation (Sandage & Katem, 1982) --- u_SK uncertain identifier flag --- Var Variable designation (Sawyer Hogg 1973, for X42 see Kholopov 1977) --- u_Var uncertain identifier flag --- Patricia Bauer CDS 1993 Sep 08 J_A+AS_104_161.xml A near infrared survey of northern planetary nebulae J/A+AS/104/169 J/A+AS/104/169 A near infrared survey of northern planetary A near infrared survey of northern planetary nebulae J P Phillips L Cuesta Astron. Astrophys. Suppl. Ser. 104 169 1994 1994A&AS..104..169P infrared: ISM: lines and bands planetary nebulae: general surveys We have observed 77 evolved planetary nebulae in the J, H, K, L', and M photometric bands. As a consequence, we note that most PN fall into a range -0.6 < (J-H)_0_ < 0.2 mag , and 0.0 < (H-K)_0_ < 1.2mag, whilst a few sources have also been detected in the range 1.0 < (K-L)_0_ < 5.3 mag . Most indices (J-H)_0_ are almost certainly depressed through the influence of HeI 2^3^ S 2^3^ P emission, whilst stellar continua appear to dominate ~ 6 sources, and components of high temperature dust enhance (J-H)_0_ in several others. Fully 60% of sources having (J-H)_0_ >=0.0 appear to be type I nebulae. Finally, we note that H_2_S(1) and Q band quadrupole emission may be important in enhancing K band fluxes for several of the nebulae, and the mean value (H-K)_0_ =~ 0.88 mag for H_2_S(1) emission sources is significantly in excess of the mean. As a consequence, the parameter (H-K)_0_ may prove a useful tool in the prior selection of nebulae having shocked, neutral gas. By contrast, the various L' band detections are likely to derive from a mix of mechanisms, including emission from grains having a broad range of temperatures.
Infrared photometry of northern planetary nebulae PK Designation in Perek & Kohoutek's catalogue --- Name Other designation of the planetary nebula --- E(B-V) Extinction mag F5GHz Flux at 5 GHz mJy Beam Beam size arcsec R Radius arcsec J J magnitude mag e_J rms uncertainty on J mag n_e_J (1) --- H H magnitude mag e_H rms uncertainty on H mag n_e_H (1) --- K K magnitude mag e_K rms uncertainty on K mag n_e_K (1) --- L' L' magnitude mag e_L' rms uncertainty on L' mag n_e_L' (1) --- M M magnitude mag e_M rms uncertainty on M mag n_e_M (1) --- ref1 short-wave references --- ref2 long-wave references --- Patricia Bauer CDS 1993 Nov 25 J_A+AS_104_169.xml Interstellar matter in Shapley-Ames elliptical galaxies. I. Multicolour CCD surface photometry J/A+AS/104/179 J/A+AS/104/179 Interstellar matter in Shapley-Ames elliptical Interstellar matter in Shapley-Ames elliptical galaxies. I. Multicolour CCD surface photometry P Goudfrooij L Hansen H E Joergensen H U Noergaard-Nielsen T De Jong L B Van Den Hoek Astron. Astrophys. Suppl. Ser. 104 179 1994 1994A&AS..104..179G galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: photometry We present accurate CCD surface photometry in Johnson B and V and Cousins I for a complete, magnitude-limited sample of 56 elliptical galaxies from the RSA catalog. For each galaxy we have determined radial profiles of surface brightness, B-V and/or B-I colour index, ellipticity, position angle, and the third- and fourth order Fourier coefficients that describe the deviations of the B, V, and I isophotes from perfect ellipses, using a full two-dimensional fitting technique. The present sample contains 13 galaxies for which no previous isophote analysis has been published, and 26 without published colour gradients. The radial profiles of the ellipticity, position angle, and the third- and fourth-order Fourier coefficients are found to show considerable detail. The profiles are mostly similar in all passbands, except in cases where dust lanes or patches are present. In this respect, the higher-order Fourier coefficients turn out to be sensitive diagnostic tools for the presence of dust in elliptical galaxies. Isophotal deviations from ellipses on the level of 0.5-1% are found to be common in elliptical galaxies. As noted before by others, these deviations are due to structures that do not necessarily align with the apparent major or minor axes of the galaxies, advocating the use of both the cosine and sine higher-order terms in correlation studies. We show that fitting outer radial intensity profiles of elliptical galaxies is an excellent tool for determining the sky background for the surface photometry. The sky values determined from a power-law fit to the outer intensity profiles are found to be within 0.1% of the sky values at the corners of present-day large CCDs where the contribution of galaxy light is negligible. The average colour gradients for the sample galaxies in B-V and B-I are 0.06 and 0.14 mag arcsec^-2^ per decade in radius, respectively. This compares well with colour gradients in elliptical galaxies found by others. The small uncertainty introduced by the sky background determination method applied here results in an average internal uncertainty of only ~ 0.01 mag for our colour gradients, which is significantly better than the results of previous studies. The profiles are compared extensively with results from other authors when available. The result is encouraging, especially for the ellipticity and position angle where we find mean RMS differences of 0.01 and 1.8deg , respectively. The surface brightness profiles generally agree to within +/- 0.0.5mag.
Basic parameters, zero points, backgrounds, colour corrections; colour indices, ellipticity, position angle and their gradients, and effective higher order residual terms (table1, 4, 5 and 6 of the paper) Name Galaxy name number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- RSA Galaxy classification taken form the RSA (Sandage & Tammann, 1981) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- RC2 Galaxy classification taken from the RC2 (de Vaucouleurs et al., 1976) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- v_grp Group velocity from Davies et al. (1987) number=1 The group velocity is corrected for the motion with respect to the centroid of the Local Group, calculated from solution No.2 of Yahil et al. (1977) km/s Dist. Assumed distance (H0 = 50 km\s\Mpc) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise Mpc BT Total blue magnitude number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag BT_0 Total blue magnitude corrected for extinction number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag M(BT_0) Absolute blue magnitude number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag r_eff Effective radius number=2 The effective radii are taken from Burstein et al. (1987) and converted to major-axis effective radii using the ellipticities measured in this paper. arcsec Env Environnement number=3 The comments on the environment have been taken mostly from the RC2. Comments denoted HG or GH indicate membership of groups listed by Huchra & Geller (1982) or Geller & Huchra (1983), respectively. The number in parentheses lists the number of galaxies in that group --- Z(B) Zero point used in the photometric calibration number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- n_Z(B) (4) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- Z(V) Zero point used in the photometric calibration number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- n_Z(V) (4) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- Z(I) Zero point used in the photometric calibration number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise -- n_Z(I) (4) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- B B sky background magnitude number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag e_B rms uncertainty on B number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag V V sky background magnitude number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag e_V rms uncertainty on V number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag I I sky background magnitude number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag u_I Uncertainty flag on I number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- e_I rms uncertainty on I number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag Bc Extinction + K correction number=5 Corrections applied to the model magnitudes for the different passbands, ie, the combination of Galactic foreground extinction and K correction --- Vc Extinction + K correction number=5 Corrections applied to the model magnitudes for the different passbands, ie, the combination of Galactic foreground extinction and K correction --- Ic Extinction + K correction number=5 Corrections applied to the model magnitudes for the different passbands, ie, the combination of Galactic foreground extinction and K correction --- B-V Average B-V colour at r_e/2 number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag e_B-V rms uncertainty on B-V number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag B-I Average B-I colour at r_e/2 number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag u_B-I Uncertainty flag on B-I number=6 The uncertainty of the sky background determination is reflected in the error estimates of the colour gradients. --- e_B-I rms uncertainty on B-I number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise mag n_B-I (6) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- D1 Logarithmic colour gradient (Delta(B-V)/Delta(log r)) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- e_D1 rms uncertainty on D1 number=7 Data with an asterisk superscript are V-I data. Data with a semicolon (:) are uncertain due to non-photometric weather during the I observations. --- D2 Logarithmic colour gradient (Delta(B-I)/Delta(log r)) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- e_D2 rms uncertainty on D2 number=7 Data with an asterisk superscript are V-I data. Data with a semicolon (:) are uncertain due to non-photometric weather during the I observations. --- n_e_D2 (6) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- epsilon Average ellipticity number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- e_epsilon rms uncertainty on epsilon number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- D3 Logarithmic gradient (Delta(epsilon)/Delta(log r)) number=8 These quantities have been derived from a fit to the V-band data from the inner cut off radius to the radius where these quantities become fixed --- e_D3 rms uncertainty on D3 number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- PA Position angle number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise d e_PA rms uncertainty on position angle number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise d D4 Logarithmic gradient (Delta(PA)/Delta(log r)) number=8 These quantities have been derived from a fit to the V-band data from the inner cut off radius to the radius where these quantities become fixed --- e_D4 rms uncertainty on D4 number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- S3 third order sine coefficient number=9 The Fourier terms S3, S4, C3, and C4 correspond to the sine and cosine 3theta and 4theta terms, where theta is the position angle with respect to the major axis of the ellipse % C3 third order cosine coefficient number=9 The Fourier terms S3, S4, C3, and C4 correspond to the sine and cosine 3theta and 4theta terms, where theta is the position angle with respect to the major axis of the ellipse % S4 fourth order sine coefficient number=9 The Fourier terms S3, S4, C3, and C4 correspond to the sine and cosine 3theta and 4theta terms, where theta is the position angle with respect to the major axis of the ellipse % C4 fourth order cosine coefficient number=9 The Fourier terms S3, S4, C3, and C4 correspond to the sine and cosine 3theta and 4theta terms, where theta is the position angle with respect to the major axis of the ellipse % r_C4 radius at which the extremum of the C4 parameter is reached. number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise arcsec n_r_C4 (10) number= Telescopes: 2.2 correspond to the 2.2-m ESO/MPI Telescope 1.54 correspond to the 1.54-m Danish Telescope 1.0 correspond to the 1.0-m Jacobus Kapteyn Telescope 0.91 correspond to the 0.91-m Dutch Telescope The scale is in arcsec/bin FV = Field of view RN = Readout noise --- Observing log Name Galaxy name number=1 N for NGC, I for IC . --- R/T Run/Telescope number=2 The observation entitled DAF was kindly taken for us by D.A. Forbes and R.C. Thomson during the night Nov. 23/24, 1990. The B observation of NGC 4374 has been described in Hansen et al. (1985). Telescopes: 0.91 correspond to 0.91-m Dutch Telescope at ESO 1.00 correspond to 1.0-m Jacobus Kapteyn Telescope at LPO 1.54 correspond to 1.54-m Danish Telescope at ESO 2.20 correspond to ESO/MPI 2.2-m telescope at ESO. --- T(B) Exposure time for B observation s n_T(B) Number of exposures --- T(V) Exposure time for V observation s n_T(V) Number of exposures --- T(I) Exposure time for I observation s n_T(I) Number of exposures --- FWHM Point Spread Function (PSF) FWHM parameter arcsec delta Ellipticity PSF parameter --- psi Position angle PSF parameter --- mu Inner cut off radius (ICOR) for the radial profile of surface brightness --- B-V ICOR for the radial profile of B-V --- B-I ICOR for the radial profile of B-I --- n_(B-I) (3) --- epsilon ICOR for the radial profile of ellipticity --- phi ICOR for the radial profile of position angle --- b photometry of NGC596 v photometry of NGC596 b photometry of NGC720 i photometry of NGC720 v photometry of NGC720 b photometry of NGC821 i photometry of NGC821 v photometry of NGC821 b photometry of NGC1395 i photometry of NGC1395 v photometry of NGC1395 b photometry of NGC1399 i photometry of NGC1399 v photometry of NGC1399 b photometry of NGC1404 i photometry of NGC1404 v photometry of NGC1404 b photometry of NGC1407 i photometry of NGC1407 v photometry of NGC1407 b photometry of NGC1427 v photometry of NGC1427 b photometry of IC1459 i photometry of IC1459 v photometry of IC1459 b photometry of NGC1537 i photometry of NGC1537 v photometry of NGC1537 b photometry of NGC1549 i photometry of NGC1549 v photometry of NGC1549 b photometry of NGC1700 i photometry of NGC1700 v photometry of NGC1700 b photometry of NGC2300 i photometry of NGC2300 v photometry of NGC2300 b photometry of NGC2325 v photometry of NGC2325 b photometry of NGC2974 i photometry of NGC2974 v photometry of NGC2974 b photometry of NGC2986 i photometry of NGC2986 v photometry of NGC2986 b photometry of NGC3136 i photometry of NGC3136 v photometry of NGC3136 b photometry of NGC3193 i photometry of NGC3193 v photometry of NGC3193 b photometry of NGC3250 i photometry of NGC3250 v photometry of NGC3250 b photometry of IC3370 i photometry of IC3370 v photometry of IC3370 b photometry of NGC3377 i photometry of NGC3377 v photometry of NGC3377 b photometry of NGC3379 i photometry of NGC3379 v photometry of NGC3379 b photometry of NGC3557 v photometry of NGC3557 b photometry of NGC3608 i photometry of NGC3608 v photometry of NGC3608 b photometry of NGC3610 i photometry of NGC3610 v photometry of NGC3610 b photometry of NGC3613 i photometry of NGC3613 v photometry of NGC3613 b photometry of NGC3640 i photometry of NGC3640 v photometry of NGC3640 b photometry of NGC3706 i photometry of NGC3706 b photometry of NGC3904 i photometry of NGC3904 b photometry of NGC3962 i photometry of NGC3962 v photometry of NGC3962 b photometry of NGC4125 i photometry of NGC4125 v photometry of NGC4125 b photometry of NGC4261 v photometry of NGC4261 b photometry of NGC4278 i photometry of NGC4278 v photometry of NGC4278 b photometry of IC4296 i photometry of IC4296 v photometry of IC4296 b photometry of NGC4365 i photometry of NGC4365 v photometry of NGC4365 b photometry of NGC4373 v photometry of NGC4373 b photometry of NGC4374 i photometry of NGC4374 b photometry of NGC4473 i photometry of NGC4473 v photometry of NGC4473 b photometry of NGC4486 i photometry of NGC4486 v photometry of NGC4486 b photometry of NGC4494 v photometry of NGC4494 b photometry of NGC4564 i photometry of NGC4564 v photometry of NGC4564 b photometry of NGC4589 i photometry of NGC4589 v photometry of NGC4589 b photometry of NGC4621 i photometry of NGC4621 v photometry of NGC4621 b photometry of NGC4660 i photometry of NGC4660 v photometry of NGC4660 b photometry of NGC4696 i photometry of NGC4696 v photometry of NGC4696 b photometry of NGC4697 i photometry of NGC4697 v photometry of NGC4697 b photometry of NGC5018 i photometry of NGC5018 v photometry of NGC5018 b photometry of NGC5044 i photometry of NGC5044 v photometry of NGC5044 b photometry of NGC5061 i photometry of NGC5061 v photometry of NGC5061 b photometry of NGC5322 i photometry of NGC5322 v photometry of NGC5322 b photometry of NGC5576 i photometry of NGC5576 v photometry of NGC5576 b photometry of NGC5813 i photometry of NGC5813 v photometry of NGC5813 i photometry of NGC6482 v photometry of NGC6482 b photometry of NGC7144 v photometry of NGC7144 b photometry of NGC7507 i photometry of NGC7507 v photometry of NGC7507 r Effective radius arcsec dr Major axis radius arcsec eps Ellipticity --- e_eps rms uncertainty on ellipticity --- pos Position angle deg e_pos rms uncertainty on position angle deg c3 Cos (3 theta) coefficient % e_c3 rms uncertainty on c3 % s3 Sin (3 theta) coefficient % e_s3 rms uncertainty on s3 % c4 Cos (4 theta) coefficient % e_c4 rms uncertainty on c4 % s4 Sin (4 theta) coefficient % e_s4 rms uncertainty on s4 % c5 Cos (5 theta) coefficient % e_c5 rms uncertainty on c5 % s5 Sin (5 theta) coefficient % e_s5 rms uncertainty on s5 % c6 Cos (6 theta) coefficient % e_c6 rms uncertainty on c6 % s6 Sin (6 theta) coefficient % e_s6 rms uncertainty on s6 % mell Magnitude integrated inside ellipse --- e_mell rms uncertainty on mell --- mcirc Magnitude integrated inside circle --- e_mcirc rms uncertainty on mcirc --- mu Local surface brightness mag/arcsec2 e_mu rms uncertainty on mu mag/arcsec2 Patricia Bauer CDS 1993 Nov 15 J_A+AS_104_179.xml Young stars associated with the Vela Molecular Ridge. I. VMR clouds C and D, Collinder 197 and Vela R2. J/A+AS/104/233 J/A+AS/104/233 Young stars associated with the Vela Molecular Young stars associated with the Vela Molecular Ridge. I. VMR clouds C and D, Collinder 197 and Vela R2. B Pettersson B Reipurth Astron. Astrophys. Suppl. Ser. 104 233 1994 1994A&AS..104..233P catalogs HII regions ISM: clouds stars: formation stars: pre-main sequence surveys An objective prism survey for H{alpha}-emission-line stars towards the HII regions RCW 27, 32 and 33 and the northwestern parts of the Vela Molecular Ridge is presented. 278 H{alpha}-emitting objects have been found and their relation to the HII regions and to dark clouds in the area is discussed. We identify what appears to be two new large associations of T Tauri stars, Vela T1 and T2, at a distance of 1 kpc. The relation of low-mass H{alpha}-emission stars with the Vela Molecular Ridge is discussed.
Positions and magnitudes for the emission-line stars ESO-Halpha Identification --- Map Identification of finding chart in figure 3 --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg l_mv limit flag on mv --- mv Photographic visual magnitude (result of iris photometry) mag I- Sign of Halpha intensity --- I Estimated Halpha emission line strength on a scale from 1 (faint) to 5 (very strong) --- Comment (1) --- Patricia Bauer CDS 1993 Nov 23 J_A+AS_104_233.xml A CCD survey of galaxies. II: observations with the 2.1 m telescope at San Pedro Martir J/A+AS/104/271 J/A+AS/104/271 A CCD survey of galaxies. II: observations A CCD survey of galaxies. II: observations with the 2.1 m telescope at San Pedro Martir G Gavazzi B Garilli L Carrasco A Boselli I Cruz-Gonzalez Astron. Astrophys. Suppl. Ser. 104 271 1994 1994A&AS..104..271G galaxies: general galaxies: spiral galaxies: photometry As a part of a CCD survey of galaxies belonging or projected onto the Coma and Hercules Superclusters and to the A262, Virgo and Cancer clusters, we present isophote maps and photometric profiles of 87 galaxies (85 taken with the V, 25 with the B and 3 with the U Johnson filters). For the objects in common we compare our results with those in the RC3.
Target galaxies CGCG CGCG denomination --- NGC NGC/IC denomination --- UGC UGC denomination --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec T morphological type --- agg aggregation parameter number=1 1-3: Coma-A1367 clusters 5-7: Coma supercluster members 8-18: foreground of Coma supercluster 19: background of Coma supercluster 30: Virgo members 35: Virgo Southern extension 40-46: groups in the Canncer cluster 47: A2147 51: A2151 97: A2197 99: A2199 --- m_pg CGCG photographic magnitude. For double systems the CGCG magnitude is given to the brightest member of the system mag a major diameter arcmin b minor diameter arcmin Vh heliocentric galaxy velocity km/s Photometric results CGCG CGCG denomination --- Filt Filter used --- Yr Observing date (year) yr PQ Photometrical quality number=1 p means obtained during photometric conditions * indicates the 26 non photometric frames which were calibrated using aperture photometry available in the literature --- sky Sky brightness mag/arcsec2 1-b/a Ellipticity of elliptical rings --- a_25 Observed major radius determined at the 25th magnitude isophote arcsec m_25 Integrated magnitude at the 25th magnitude isophote mag m_-0.5 Integrated magnitude at the radius a25/3 mag c_31 Concentration index --- Patricia Bauer CDS 1993 Oct 22 J_A+AS_104_271.xml A new catalogue of members and candidate members of the Herbig Ae/Be (HAEBE) stellar group J/A+AS/104/315 J/A+AS/104/315 Member of Herbig Ae/Be stellar group A new catalogue of members and candidate members of the Herbig Ae/Be (HAEBE) stellar group P S The D de Winter M R Perez Astron. Astrophys. Suppl. Ser. 104 315 1994 1994A&AS..104..315T Stars, Be catalogs infrared: stars stars: emission-line, Be stars: formation stars: pre-main sequence An up-to-date catalogue of Herbig Ae/Be (HAEBE) stars and related objects is listed in five tables, containing 287 objects. Table 1 contains all Ae and Be stars which historically are recognized as true HAEBE stars or potential candidate members. Table 2 gives the stars of spectral type Fe, and emission line stars with very uncertain or unknown spectral type. In Table 3 are given all known Extreme Emission Line Objects (EELOs), of which most have not been identified to belong to any specific group. Table 4a and b list other Bep or B[e] stars with strong IR-excess and unknown spectral type. Table 5 contains the non-emission line possible young objects. Furthermore, Table 6 contains 35 stars rejected from former published lists of HAEBE stars. In these tables we are including coordinates, spectral types, visual magnitudes, ranges in photometric variability and references of several key publications related to each object. Relevant remarks, such as the presence of a nebula in the vicinity of an object, are also given.
Stars of which the optical and IRAS coordinates are offsetted by >= 30" Name Optical source name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec IRAS IRAS source --- RA.IRASh Right ascension 1950 from IRAS h RA.IRASm Right ascension 1950 from IRAS min RA.IRASs Right ascension 1950 from IRAS s DE.IRAS- Declination sign from IRAS --- DE.IRASd Declination 1950 from IRAS deg DE.IRASm Declination 1950 from IRAS arcmin DE.IRASs Declination 1950 from IRAS arcsec Herbig Ae/Be members and candidate members F-type PMS stars, potential candidates and those with unknown spectral type Extreme emission line objects (EELOs) Other early type emission line stars with IR-excess from AIS </tableLink> <tableLink xlink:href="table5.dat"> <title>Non-emission line early type shell stars and young stellar candidates Emission line stars rejected as Herbig Ae/Be candidates Name Name of the star --- Cat Catalogue designation number=1 see details on the various designations in file "liste2.txt" --- RAh Right ascension 1950 (as obtained from HeB, the IRAS PSC or SIMBAD) h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 (taken from HeB, the IRAS PSC or SIMBAD) deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec u_DEs Uncertainty flag on declination, * denotes a precision of the order of arcmin --- PR faintest magnitude of the photometric range mag PR2 brightest magnitude of the photometric range mag n_PR Type of magnitude number=2 The largest photometric range known from published data. B, V, R and I indicate that the given magnitudes were obtained by using filters of the Johnson-Cousins UBVRI system pg indicates photographically measured magnitudes K indicates that magnitudes are measured through the 2.2 micrometer filter of the Johnson JHKLM system. --- Vmag Visual magnitude or faintest visual magnitude (if range of magnitude)(3) mag Vmag2 brightest visual magnitude if range of magnitude mag u_Vmag 'd' indicates a bracketed value --- Sp Spectral characteristics number=4 The spectral characteristics, such as spectral type, luminosity class, emission lines (e) in the optical spectrum and the detection of a shell (sh) spectrum, are given. If several spectral types are known, they are separated by a slash. Note that the determination of the spectral type depends on the studied wavelength region, and is influenced by the variability in the spectral lines. We also like to mention that a clear distinction between Beq or Bep objects has not been made. However, in some cases the historically employed classification is given. --- Other Other designation number=5 The other designations are listed in alphabetic order with a maximum of three. They are given to avoid confusions with other identifications, and for the reader's convenience, in cases when different names are frequently used in the literature. The abbreviations are explained below. When any confusion exists about the possible optical identification of an IRAS source, or when different designations refer to the same optical object, they are separated by the notation =?, followed by the name of the source. --- IRAS IRAS source number=6 Listed are the confirmed detections of IRAS at or near the optically identified source. The source of the data is given behind the abbreviation used which are: N: No IRAS source Y: Iras source. ?: IRAS detection hole, see Weintraub 1990 O: Offset between optical- and IRAS-source --- Neb Nebula number=7 When it is known that the star is associated with a nebula, it is indicated by the letter Y (Yes), otherwise by the letter N (No). For unknown cases, the entries in the column are empty. The references from which the listed informations are obtained are given behind these letters. --- Rem Remarks number=8 Any special remark found in the literature, such as near-IR excess, degree of linear polarization, detection of a nearby companion or of binarity, and the evolutionary status of an object, is given. The remarks and their references are separated by a dash. Abbreviations used in the remarks: Bin: Binary Cand: Candidate Class Be: Classical Be-star Comp: Companion DST: Double star Ecl Bin: Eclipsing Binary Em: Emission HHO: Herbig-Haro object HP(I): High (Intrinsic) Pol, 1-3% L_*: Stellar luminosity LBV: Luminous Blue Variable LP(I): Low (Intrinsic) Pol, <= 1% NIRE: Near Infrared Excess N PN: No Planetary Nebula Neb: Nebula Obs Reg: Obscured Region PN: Planetary Nebula Pol: Polarization Poss: Possible Ref Neb: Reflection Nebula Reg: Region Rej: Rejected see sect. 3.3. and Table 2. Sc: Source Sp T: Spectral Type Symb: Symbiotic star Var: Variable VHP(I): Very High (Intrinsic) Pol, >= 3% The numbered remarks mean the following: (1) Sp. char. XY Per w=Aep+sh (2) Refl. Neb-HeB, DST?-FiM (3) Neb like star-HeB (4) High L_*+PN?+Ring Neb-HeB (5) No IRAS sc-BeC (6) Triangle Neb-HeB (7) Bin?-FiM (8) Close to LSS 3027A=CPD-61 3587-SeE (9) HAEBE? or B[e]? (10) in Obs Reg-HeR (11) N PN+HII Reg-ArC (12) Neb or Star?-HeB (13) No IRAS sc-BeC (14) Two faint Comps-HeR (15) On edge of small dark cloud-HeB (16) No IRAS sc-BeC (17) N PN+Symb?-ArC, LBV?-SoB (18) Norm. Be?-HeB The references are indicated by a 3-letter detailed in the "References in the tables" section below. --- Refs Other references number=9 Additional references of the objects mentioned in other columns. All the references indicate the published lists where the star has been quoted and the ones which are used to collect the given information. The references are indicated by a 3-letter detailed in the "References in the tables" section below. --- liste2.txt Abbreviations of the objects designations Patricia Bauer CDS 1993 Dec 06 J_A+AS_104_315.xml Evolutionary sequences of stellar models with new radiative opacities. III. Z=0.0004 and Z=0.05 J/A+AS/104/365 J/A+AS/104/365 Evolutionary sequences of stellar models with new Evolutionary sequences of stellar models with new radiative opacities. III. Z=0.0004 and Z=0.05 F Fagotto A Bressan G Bertelli C Chiosi Astron. Astrophys. Suppl. Ser. 104 365 1994 1994A&AS..104..365F Hertzsprung-Russell (HR diagram) stars: abundances stars: evolution stars: interiors We present detailed tabulations of two large grids of stellar models with the extreme initial chemical composition [Z=0.0004, Y=0.230], and [Z=0.050, Y=0.352]. The models are computed with the most recent radiative opacities (OPAL) by Iglesias et al. (1992) and with the inclusion of overshoot from convective cores and envelopes according to the formalism by Bressan et al. (1981) and Alongi et al. (1991), respectively, and the revision made by Bressan et al. (1993a). These calculations represent the continuation of the series initiated with the paper by Bressan et al. (1993a) for the grid with [Z=0.020, Y=0.280] (the reference solar like abundance). The tracks are calculated for a wide range of initial masses from 0.6 M_{sun}_ to 120 M_{sun} _ and extend from the ZAMS till very advanced evolutionary phases. Specifically, low and intermediate mass stars are followed to the beginning of the TP-AGB, while massive stars are followed till the core C-ignition. The models of low and intermediate mass stars are calculated at constant mass, whereas those of massive stars are followed in presence of mass loss by stellar winds incorporating a suitable dependence on the metallicity. The results of all the models are given in extensive tables which summarize also the lifetimes of the various phases and the variations of surface abundances by dredge-up phenomena and mass loss by stellar wind. The salient features brought by the different metallicity and helium content are briefly outlined, with particular attention to the anomalous behaviour of the low mass, high metallicity stars in core He-burning and later phases. Such grids of evolutionary tracks are well indicated for studies of population synthesis in virtue of their large coverage of masses, evolutionary phases, and chemical composition. The high metallicity set is particularly suited to interpret the stellar content of bulges and elliptical galaxies.
Evolutionary sequences of low mass stars up to the tip of the RGB. 0.6 < M < 1.7 for z=0.0004 Evolutionary sequences of low mass stars up to the tip of the RGB. 0.6 < M < 1.7 for z=0.05 Evolutionary sequences of low mass stars during the core helium-burning and EAGB phases. 0.5 < M < 1.7 for z=0.0004 Evolutionary sequences of low mass stars during the core helium-burning and EAGB phases. 0.5 < M < 1.7 for z=0.05 Evolutionary sequences of intermediate stars up to the TPAGB or carbon-ignition. 1.8 < M < 9.0 for z=0.0004 Evolutionary sequences of intermediate stars up to the TPAGB or carbon-ignition. 1.8 < M < 9.0 for z=0.05 m Initial mass Sun Age Age of models yr log(L) Total luminosity Sun log(Teff) Effective temperature K log(G) Surface gravity cm/s2 log(Tc) Central temperature K log(rho_c) Central density g/cm3 COMP Central abundance (by mass) of hydrogen or helium --- X_C Central abundance of 12C --- X_O Central abundance of 16O --- Conv Fractionary mass of the convective core (inclusive of overshoot) --- Q_disc Fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log(L_H) Hydrogen luminosity Sun Q1_H Fractionary mass of the inner border of the hydrogen rich region --- Q2_H Fractionary mass of the outer border of the H-burning region. The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- log(L_He) Helium luminosity Sun Q1_He Fractionary mass of the inner border of the He-burning region (when greater than zero He-burning is in a shell). The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- Q2_He Fractionary mass of the upper border of the He-burning region. The boundary is taken as above. --- log(L_C) Carbon luminosity Sun log(L_nu) Neutrinos luminosity (absolute value) Sun Q_Tmax Fractionary mass of the point where the temperature attains the maximum value --- Evolutionary sequences for massive stars. 12 < M < 120 for z=0.0004 Evolutionary sequences for massive stars. 12 < M < 120 for z=0.05 m Initial mass Sun Age Age of models yr M Current value of the mass Sun log(L) Total luminosity Sun log(Teff) Effective temperature K log(G) Surface gravity cm/s2 log(Tc) Central temperature K log(rho_c) Central density g/cm3 COMP Central abundance of hydrogen or helium (by mass) --- X_C Central abundance of 12C --- X_O Central abundance of 16O --- Conv Fractionary mass of the convective core (inclusive of overshoot) --- Q_disc Fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log(L_H) Hydrogen luminosity Sun Q1_H Fractionary mass of the inner border of the hydrogen rich region --- log(L_He) Helium luminosity Sun log(M_dot) Absolute value of the mass loss rate Sun/yr X_sur Surface abundance (by mass) of 1 H --- Y_sur Surface abundance (by mass) of 4 He --- XC_sur Surface abundance (by mass) of 12 C --- XN_sur Surface abundance (by mass) of 14 N --- XO_sur Surface abundance (by mass) of 16 O --- tabz0004.tex LaTex version of the tables for z=0.0004 tabz05.tex LaTex version of the tables for z=0.05 Patricia Bauer CDS 1993 Dec 13 J_A+AS_104_365.xml Integrated photometric properties of open clusters J/A+AS/104/379 J/A+AS/104/379 Integrated Photometry of open clusters Integrated photometric properties of open clusters P Battinelli A Brandimarti R Capuzzo-Dolcetta Astron. Astrophys. Suppl. Ser. 104 379 1994 1994A&AS..104..379B Clusters, open Photometry open clusters and associations: general techniques: photometric Galactic open clusters provide an abundant sample of stellar aggregates of various sizes, ages and metal abundances, apt to constitute a template for comparison with star systems in other galaxies. In this paper we present and discuss a standard methodology to synthesize U,B,V fluxes and colours, and apply it to a set of 138 open clusters. Results are compared with previous ones available in the literature. We were able to calibrate a mass-luminosity relation by which we evaluated the mass of ~ 400 open clusters, leading to a well defined present-day mass function. The number-complete sample of galactic open clusters presented in Battinelli & Capuzzo-Dolcetta (1992AJ....103.1596B) is enlarged of a 15%.
Magnitude, colour and mass Name Open cluster name Bas=Basel, Ber=Berkeley, Bla=Blanco, Boc=Bochum, Byu=Byurakan, Col=Collinder, Fei=Feinstein, Hog=Hogg, Hya=Hyades, Lyn=Lynga, Mar=Markarian, N=NGC, Pis=Pismis, Ple=Pleiades, Ros=Roslund, Rup=Ruprecht, Tra=Trapezium, Upg=Upgren, VdH=van den Bergh & Hagen, Wat=Waterloo, Wes=Westerlund. --- n Number of members stars --- Mv Integrated magnitude mag (B-V)0 (B-V)0 colour in decimal log mag (U-B)0 (U-B)0 colour in decimal log mag logM Mass in decimal log [solMass] Notes Notes on integrated photometry The symbols refer to other authors who give integrated photometry: b= Spassova N.M. & Baev P.V. =1985Ap&SS.112..111S g= Gray D.F. =1965AJ.....70..362G l= Lynga G. 1987, Lund Catalogue of Open Cluster Data, 5th ed., CDS Catalogue <V/92> p= Pandey A.K., Bhatt B.C., Mahra H.S. & Sagar R. =1989MNRAS.236..263P s= Sagar R., Joshi U.C. & Sinvhal S.D. 1983, Bull. Astron. Soc. India 11, 44 Symbol c stands for clusters in the "complete" sample and symbol : stands for uncertain values. Hog 17 is included in the sample due to BCD determination based on a higher number of members (41). --- r_Notes Comma-separated references, see file refs.dat --- References to table1 RefNo Reference number --- BibCode Coded Reference --- Text Text of reference --- Galactic coordinates, distance and age Name Open cluster name Bas=Basel, Ber=Berkeley, Bla=Blanco, Boc=Bochum, Byu=Byurakan, Col=Collinder, Fei=Feinstein, Hog=Hogg, Hya=Hyades, Lyn=Lynga, Mar=Markarian, N=NGC, Pis=Pismis, Ple=Pleiades, Ros=Roslund, Rup=Ruprecht, Tra=Trapezium, Upg=Upgren, VdH=van den Bergh & Hagen, Wat=Waterloo, Wes=Westerlund. --- GLON Galactic longitude l deg GLAT Galactic latitude b deg d Projected distance to the Sun pc z Height on the galactic plane pc D Angular diameter arcmin Log(t) Logarithmic age [yr] (B-V)to Turn-off colour mag E(B-V) Reddening mag Patricia Bauer, Francois Ochsenbein CDS 1999 Jan 24 UNKNOWN UNKNOWN * 18-Jan-1994: first archived at CDS (Patricia Bauer) * 24-Jan-1999: references added (Francois Ochsenbein) J_A+AS_104_379.xml A large, complete, volume-limited sample of G-type dwarfs. I. Completion of Stroemgren uvby photometry J/A+AS/104/429 J/A+AS/104/429 A large, complete, volume-limited sample of G-type A large, complete, volume-limited sample of G-type dwarfs. I. Completion of Stroemgren uvby photometry E H Olsen Astron. Astrophys. Suppl. Ser. 104 429 1994 1994A&AS..104..429O Galaxy: evolution solar neighborhood stars: fundamental parameters stars: late-type surveys techniques: photometric Four-colour photometry of potential dwarf stars of types G0 to K2, selected from the Michigan Spectral Catalogues (Vol. 1-3), has been carried out. The results are presented in a catalogue containing 4247 uvby observations of 3900 stars, all south of {delta} = -26deg. The overall internal rms errors of one observation (transformed to the standard system) of a program star in the interval 8.5 < V < 10.5 are 0.0044, 0.0021, 0.0039, and 0.0059, respectively, in V, b-y, m_1_ , and c_1_. The purpose of the catalogue, combined with earlier catalogues, is to allow selection of a large, complete, volume-limited sample of G- and K-type dwarfs, investigate their metallicity distribution, and compare it to predictions of various models of galactic chemical evolution. Future papers in this series will discuss these subjects.
60 uvby standards, standard system HD HD (Henry Draper) designation --- Mult Identification of visual double star components included in the diaphragm --- V transformed to the standard Johnson V mag. mag e_V mean error on V mag b-y b-y mag e_(b-y) mean error on (b-y) mag m1 = (v-b) - (b-y) mag e_(m1) mean error on m1 mag c1 = (u-v) - (v-b) mag e_(c1) mean error on c1 mag w_V weight of V --- w_col weight of 4-colour indices --- NN Number of nights --- D(V) Difference V(standard) - V(transformed) mag D(b-y) Difference (b-y)(st) - (b-y)(tr) mag D(m1) Difference m1(st) - m1(tr) mag D(c1) Difference c1(st) - c1(tr) mag The catalogue HD ? HD (Henry Draper) designation NB!: This column may be blank --- Mult Identification of visual double star components included in the diaphragm --- Prog Program star list K = G or K-type star (see paper,section 2.1.1) B = Calibration star (see paper,section 2.1.1) M = G or K giant (see paper, section 2.1.2) * = miscellaneous reasons --- DM Durchmusterung identification (BD, CD or CP in bytes 17-18; SZZNNNNN on bytes 19-26; appended letter in byte 27 NB! This column may be blank --- ID Alternative identification --- T Transformation group (see paper!, section 3.4.2) D = GKV group, G or C = GKIII group, % W or blank = BAF group --- V transformed to the standard Johnson V mag. mag e_V mean error on V mag b-y on standard system if byte 39 is D mag e_(b-y) mean error on (b-y) mag m1 on standard system if byte 39 is D mag e_(m1) mean error on m1 mag c1 on standard system if byte 39 is D mag e_(c1) mean error on c1 mag w_V weight of V --- w_col weight of 4-colour indices --- NN Number of nights --- Note N = visual double star not listed in IDS D = calibration star (see paper,section 2.1.1) G = G or K giant (see paper, section 2.1.2) * = individual note (see paper) --- Erik Heyn Olsen CDS 1994 Mar 19 Erik H. Olsen <eho@bro835.astro.ku.dk> J_A+AS_104_429.xml Stark broadening of hydrogen Lyman and Balmer lines in the conditions of stellar envelopes J/A+AS/104/509 J/A+AS/104/509 Stark broadening of hydrogen Lyman and Balmer line Stark broadening of hydrogen Lyman and Balmer lines in the conditions of stellar envelopes C Stehle Astron. Astrophys. Suppl. Ser. 104 509 1994 1994A&AS..104..509S atomic data atomic processes line: profiles Tables of Stark broadened hydrogen lines of the Lyman and Balmer series are presented under the conditions of stellar envelopes. The formalism is based on the Model Microfield Method (MMM) for both the electronic and ionic contributions to the line shape.
Lyman alpha (1-2) H+, He+ and Ar+ perturbers (lambda = 1215.68, Kalpha = 6.731E-06) Lyman beta (1-3) H+, He+ and Ar+ perturbers (lambda = 1025.73, Kalpha = 3.587E-05) Lyman gamma (1-4) H+, He+ and Ar+ perturbers (lambda = 972.55, Kalpha = 7.965E-05) Lyman delta (1-5) H+, He+ and Ar+ perturbers (lambda = 949.75, Kalpha = 1.563E-04) Lyman epsilon (1-6) H+, He+ and Ar+ perturbers (lambda = 937.81, Kalpha = 2.651E-04) Lyman (1-7) H+, He+ and Ar+ perturbers (lambda = 930.76, Kalpha = 4.212E-04) Lyman (1-8) H+, He+ and Ar+ perturbers (lambda = 926.24, Kalpha = 6.238E-04) Lyman (1-9) H+ perturbers (lambda = 923.16, Kalpha = 8.885E-04) Lyman (1-10) H+ perturbers (lambda = 65 Kalpha = 6.731E-06) Lyman (1-11) H+ perturbers (lambda = 919.36, Kalpha = 1.616E-03) Lyman (1-12) H+ perturbers (lambda = 918.14, Kalpha = 2.093E-03) Lyman (1-13) H+ perturbers (lambda = 917.19, Kalpha = 2.662E-03) Lyman (1-14) H+ perturbers (lambda = 916.44, Kalpha = 3.319E-03) Balmer alpha (2-3) H+, He+ and Ar+ perturbers (lambda = 6564.70, Kalpha = 2.564E-03) Balmer beta (2-4) H+, He+ and Ar+ perturbers (lambda = 4862.74, Kalpha = 7.062E-03) Balmer gamma (2-5) H+, He+ and Ar+ perturbers (lambda = 4341.73, Kalpha = 1.189E-02) Balmer delta (2-6) H+, He+ and Ar+ perturbers (lambda = 4102.94, Kalpha = 1.944E-02) Balmer epsilon (2-7) H+, He+ and Ar+ perturbers (lambda = 3971.24, Kalpha = 2.948E-02) Balmer (2-8) H+ perturbers (lambda = 3890.19, Kalpha = 4.302E-02) Balmer (2-9) H+ perturbers (lambda = 3836.51, Kalpha = 6.190E-02) Balmer (2-10) H+ perturbers (lambda = 3799.01, Kalpha = 8.344E-02) Balmer (2-2) H+ perturbers (lambda = 3771.74, Kalpha = 1.094E-01) Balmer (2-12) H+ perturbers (lambda = 3751.25, K = 1.407E-01) Balmer (2-13) H+ perturbers (lambda = 3735.47, K = 1.774E-01) Balmer (2-14) H+ perturbers (lambda = 3723.03, Kalpha = 2.202E-01) Ne Electron density cm-3 Delta Dlambda/Dalpha --- T Temperature K R0/Debye ratio of the mean interelectronic distance to the electronic Debye length number=1 R0/Debye is expressed in electrons --- Dalpha Detuning from line center (2), number=3 The intensities are expressed in 1/alpha where alpha= lambda0/F0, lambda0 is the wavelength of the line center, in Angstroems F0 is the normal Holstmark field strength value in ues units: F0= 1.25 E-9 Ne**(2/3), Ne is the electronic density expressed in cm-3 "alpha" IDH+ Intensity (with Doppler), H+ perturbers number=3 The intensities are expressed in 1/alpha where alpha= lambda0/F0, lambda0 is the wavelength of the line center, in Angstroems F0 is the normal Holstmark field strength value in ues units: F0= 1.25 E-9 Ne**(2/3), Ne is the electronic density expressed in cm-3 1/"alpha" ISH+ Intensity (Stark only), H+ perturbers number=3 The intensities are expressed in 1/alpha where alpha= lambda0/F0, lambda0 is the wavelength of the line center, in Angstroems F0 is the normal Holstmark field strength value in ues units: F0= 1.25 E-9 Ne**(2/3), Ne is the electronic density expressed in cm-3 1/"alpha" IDHe+ Intensity (with Doppler), He+ perturbers number=3 The intensities are expressed in 1/alpha where alpha= lambda0/F0, lambda0 is the wavelength of the line center, in Angstroems F0 is the normal Holstmark field strength value in ues units: F0= 1.25 E-9 Ne**(2/3), Ne is the electronic density expressed in cm-3 1/"alpha" ISHe+ Intensity (Stark only), He+ perturbers number=3 The intensities are expressed in 1/alpha where alpha= lambda0/F0, lambda0 is the wavelength of the line center, in Angstroems F0 is the normal Holstmark field strength value in ues units: F0= 1.25 E-9 Ne**(2/3), Ne is the electronic density expressed in cm-3 1/"alpha" IDAr+ Intensity (with Doppler), Ar+ perturbers(3) 1/"alpha" ISAr+ Intensity (Stark only), Ar+ perturbers number=3 The intensities are expressed in 1/alpha where alpha= lambda0/F0, lambda0 is the wavelength of the line center, in Angstroems F0 is the normal Holstmark field strength value in ues units: F0= 1.25 E-9 Ne**(2/3), Ne is the electronic density expressed in cm-3 1/"alpha" Patricia Bauer CDS 1994 Jan 04 UNKNOWN UNKNOWN 04-Jan-1994: First preparation 10-May-1994: Correction in tabl1-3 (call from Chantal Stelhe) Last row with Ne=1.000E+15, T=1.000E+04: values of Dalpha, IDH+ and ISH+ were erroneous. J_A+AS_104_509.xml Search and redshift survey for IRAS galaxies behind the Northern Milky Way. J/A+AS/104/529 J/A+AS/104/529 IRAS galaxies behind the Milky Way Search and redshift survey for IRAS galaxies behind the Northern Milky Way. T Takata T Yamada M Saito P Chamaraux I Kazes Astron. Astrophys. Suppl. Ser. 104 529 1994 1994A&AS..104..529T II/174 : IRAS 2Jy Redshift Survey Data File VII/140 : Catalog of Galaxies behind the Milky Way (Saito et al., 1992) Bottinelli et al. (1992) A&AS 93, 173 =1992A&AS...93..173B Chamaraux et al. (1990) A&A 229 340 =1990A&A...229..340C Dreyer 1908 MNRAS 59, 105 =1908MmRAS..59..105D Huchtmeier & Richter 1989 A General Catalog of HI Observations of Galaxies New York: Springer-Verlag Lu et al. (1990) ApJ 357, 388 =1990ApJ...357..388L Martin et al. (1990) A&A 235, 41 =1990A&A...235...41M Mathewson, Ford & Buchhorn (1992) ApJS 81, 413 =1992ApJS...81..413M Palumbo et al. 1983 =CDS Catalogue: <VII/99> Saito et al., 1991b Catalog of Galaxies behind the Milky Way =CDS Catalogue: <VII/140> Strauss et al. (1992b) ApJS 83, 29 =CDS Catalogue: <II/174> Strauss et al. (1993) private communication Weinberger (1980) A&AS 40, 123 =1980A&AS...40..123W Yamada & Saito (1993) PASJ 45, 25 =1993PASJ...45...25Y Yamada et al. (1994) MNRAS, 270, 93 =1994MNRAS.270...93Y de Vaucouleurs et al. 1991 =CDS Catalogue: <VII/155> Galaxies, IR Redshifts galaxies: distances and redshifts infrared: galaxies large-scale structure of universe surveys We made a search for IRAS galaxies behind the Northern Milky Way by infrared selection using IRAS Point Source Catalog and visual inspection on POSS (Palomar Observatory Sky Survey) paper prints, and carried out a redshift survey of the identified objects. This paper presents a catalog of 649 IRAS galaxies with f_60_>=0.6Jy between l=150deg and 240deg at |b|<=15deg, which contains 254 newly identified galaxies and 188 newly measured radial velocities. Due to galactic extinction, our sample is a lower limit sample of the flux limited sample of IRAS galaxies, but it can give some information on the distribution of galaxies in the region perpendicular to the Supergalactic Plane. We confirm two regions with enhanced density at l~160deg, cz~5000km/s and l~190deg, cz~5000km/s and at least two possible voids.
IRAS
Catalogue of IRAS galaxies with F60>=0.6Jy IRAS IRAS name --- GLON Galactic longitude deg GLAT Galactic latitude deg F60 Flux density at 60um Jy l_F60 Limit flag (L for lower limit) on F60 --- F100 Flux density at 100um Jy l_F100 Limit flag (L for lower limit) on F100 --- OptId Optical identification number=1 G: galaxy G?: possible galaxy ?: extended image but unlike normal spiral galaxy --- MType Apparent morphological type of galaxy number=2 S: spiral E: elliptical galaxy E/S: not classified alternatively ?: irregular appearance --- MajDiam Diameter of major axis of image number=3 Diameters measured on POSS E (red) prints or UK Schmidt Atlas (I or J) film copies. (1 mm corresponds to 67 arcsec in angular size) mm MinDiam Diameter of minor axis of image number=3 Diameters measured on POSS E (red) prints or UK Schmidt Atlas (I or J) film copies. (1 mm corresponds to 67 arcsec in angular size) mm Atlas Schmidt Atlas on which the galaxy was visually identified number=4 I and J indicate the UK Schmidt I and J film copies, respectively, and blank means POSS I and E paper prints. --- Com Comments on multiplicity and image appearance number=5 For multiplicity: pair: two galaxies are located within a separation as wide as the galaxy sizes tri: triplet quar: quartet int: two galaxies appear to be interacting For image appearance: PN? : possible planetary nebula star?: possible star LSB : Low Surface Brightness HSB : High Surface Brightness ND : Nuclear Dominated pec : peculiar neb? : possible reflection nebula cD : cD galaxy --- cz Heliocentric radial velocity km/s r_cz Reference for cz velocity number=6 Reference numbers are: 1: Third Reference Catalogue of Bright Galaxies (de Vaucouleurs et al. 1991) <VII/155> 2: A General Catalog of HI Observations of Galaxies (Huchtmeier & Richter 1989) 3: Catalog of Radial Velocities of Galaxies (Palumbo et al. 1983) <VII/99> 4: Strauss et al. (1992b) <II/174> 5: Chamaraux et al. (1990A&A...229..340C) 6: Lu et al. (1990ApJ...357..388L) 7: Martin et al. (1990A&A...235...41M) 8: Mathewson, Ford & Buchhorn (1992ApJS...81..413M) 9: Bottinelli et al. (1992A&AS...93..173B) 10: "1.2 Jy Sample" by Strauss et al. (1993) A1: measurement at OAO by us A2: measurement at OAO by Yamada & Saito (1993PASJ...45...25Y) A3: measurement at Nancay by us A4: measurement at Mt. Strombolo by Yamada et al. (1994MNRAS.270...93Y) The number of 'A1' galaxies is 197, 'A2' 20, 'A3' 17 and 'A4' 1. --- CrossId Cross identification number=7 If the redshift has been known before our measurement, the heliocentric radial velocity and the reference are denoted in parenthesis. When the galaxy has two or more catalog names, only the first one is written in full name. U = UGC: Uppsala General Catalogue of Galaxies <VII/26> E = ESO: ESO/Uppsala Survey of the ESO(B) Atlas <VI/30> Z = CGCG: Catalogue of Galaxies and of Clusters of Galaxies <VII/49> M = MCG: Morphological Catalog of Galaxies <VII/62> NGC = New General Catalogue of Galaxies <VII/118> I = Index Catalogue (Dreyer 1908) (1908MmRAS..59..105D) W = Catalog of Weinberger (1980A&AS...40..123W) CGMW = Catalogue of Galaxies behind the Milky Way <VII/140> A = Anonymous galaxy taken from Huchtmeier & Richter (1989) Lu(Arecibo) = newly identified galaxy at Arecibo by Lu et al. (1990ApJ...357..388L) Martin(Nancay) = newly identified galaxy at Nancay by Martin et al. (1990A&A...235...41M) 1.936 Jy sample = newly identified galaxies by Strauss et al. (1992b)'s 1.936 Jy redshift survey <II/174> Incomplete = newly identified galaxies by Strauss et al. (1992b)'s 1.936 Jy redshift survey <II/174> 1.2 Jy sample = newly identified galaxies by Strauss et al. (1993) which have been unpublished Blanks means newly identified object in the present search on POSS and Yamada et al.'s Southern Milky Way search. The total number of blank is 283, of which 254 were found on POSS, and there are 101 objects of the 283 without radial velocities. --- Patricia Bauer CDS 1996 Aug 23 Thanks are due to Koichi Nakajima, who asked for the data. J_A+AS_104_529.xml uvby-beta photometry of Orion population stars and related objects associated with six galactic star-forming regions J/A+AS/104/557 J/A+AS/104/557 uvby-beta photometry in star-forming regions uvby-beta photometry of Orion population stars and related objects associated with six galactic star-forming regions L Terranegra C Chavarria-K S Diaz D Gonzalez-Patino Astron. Astrophys. Suppl. Ser. 104 557 1994 1994A&AS..104..557T dust, extinction stars: emission-line, Be stars: pre-main sequence Homogeneous uvby{beta} photometry of 150 stars associated with the star forming regions Taurus-Auriga, Orion, Canis Mayoris, Ophiuchus, Serpens and Cygnus, is presented here. We also present uvby{beta} photometry of 10 Herbig Ae/Be stars not belonging to the specific regions studied here. Using the (V,b-y), ({beta},[m1]), ([c1],[m1]) and ([u-b], T_eff_) diagrams we study the photometric properties of the sample. The effects of duplicity, stellar rotation, and interstellar extinction on the location in the magnitude-color and color-color diagrams of our program stars are briefly investigated. We derive reliable photometric spectral types and discuss membership to the regions and to the Orion population, as well as peculiarities of the individual stars. We also find new B stars associated with the CMa R1 star forming region and new intermediate-low mass PMS members associated with the BD+404124/BD+413731 region. The FU-Orionis stars Z CMa, V1515 Cyg and V1057 Cyg have a peculiar position in the reddening free ({beta},[m1]) diagram. With diagrams such as (V-M _v_-5 log r+5) vs. E(b-y), E(c1) vs. E(b-y), E(m1) vs. E(b-y) and E(u-b) vs. E(b-y) we investigate the IS extinction law towards the star-forming regions. We find that the total to selective extinction ratio to these regions is steeper than normal with R_y_=5.4 (R_v_=4.0) and the coefficients E(c1)/E(b-y) and E(m1)/E(b-y) used to define the reddening free indices [c1] and [m1] should be numerically smaller than the generally adopted values.
Mean uvby-beta photometry of 150 Orion population stars Group Group number number=1 See note (1) for table3b --- Name Star name --- Sp Photometric spectral type --- Note Note --- Vmag V magnitude mag e_Vmag rms uncertainty on V mag (b-y) (b-y) index mag e_(b-y) rms uncertainty on (b-y) mag c1 c1 index mag e_c1 rms uncertainty on c1 mag m1 m1 index mag e_m1 rms uncertainty on m1 mag beta beta index mag n_beta When *, the stars was not observed in Beta index --- e_beta rms uncertainty on Beta mag Nobs Number of observations --- Complete uvby-beta photometry of 150 Orion population stars Group Group number number=1 1 = Taurus-Auriga 2 = Orion 3 = CMa R1 4 = NGC 6611 5 = Ophiuchus 6 = BD+40 4124 and BD+41 3731 groups 7 = NGC 7000/IC 5070 8 = Miscellaneous stars 9 = Miscellaneous Herbig Ae/Be stars --- Name Star name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Sp Photometric spectral type --- Vmag V magnitude mag (b-y) (b-y) index mag c1 c1 index mag m1 m1 index mag beta beta index mag JDhel Heliocentric Julian day d Patricia Bauer, Francois Ochsenbein CDS 1995 Jul 07 UNKNOWN UNKNOWN * 18-Feb-1994: first prepared * 07-Jul-1995: replaced 2440000-offset dates by complete ones J_A+AS_104_557.xml Non-variability of the fine-structure constants over cosmological time scale J/A+AS/104/89 J/A+AS/104/89 Non-variability of the fine-structure constants Non-variability of the fine-structure constants over cosmological time scale A Y Potekhin D A Varshalovich Astron. Astrophys. Suppl. Ser. 104 89 1994 1994A&AS..104...89P catalogs cosmology: miscellaneous quasars: absorption lines quasars: general A statistical analysis of fine splitting of C IV, N V, O VI, Mg II, Al III and Si IV doublet absorption lines in quasar spectra is carried out in order to estimate a possible time variation of the fine-structure constant {alpha}= e^2^(h/2{pi})c (~1/137) over cosmological time scales t~10^10^yr. The observational basis of the analysis is a catalogue of 1414 pairs of wavelengths with redshifts z = 0.2 - 3.7, compiled from data published in 1980-1992. Robust statistical estimates like the ``trimmed mean'' are used as well as the least squares. No statistically significant time variation of {alpha} is found. The estimate {alpha}^-1^d{alpha}/dz = (-0.6+/-2.8)10^-4^ is obtained. For the 95% significance level, an upper bound on the rate of a relative variation of the fine-structure constant is |{alpha}^-1^d{alpha}/dz| < 5.6x10^-4^, which corresponds approximately to |{alpha}^-1^d{alpha}/dt| < 4x10^-14^ yr^-1^. This limit represents the strongest up-to-date restriction on the possible time variation of {alpha} for the epoch 0.2 <= z <~ 4.
C IV absorption wavelengths N V absorption wavelengths O VI absorption wavelengths Mg II absorption wavelengths Al III absorption wavelengths Si IV absorption wavelengths QSO QSO number --- z redshift --- lambda1 Observed wavelength 0.1nm n_lambda1 When a, air wavelength, else the wavelength is vacuum heliocentric --- lamdba2 Observed wavelength 0.1nm n_lambda2 When a, air wavelength, else the wavelength is vacuum heliocentric --- ref Reference --- Y Observational estimate of Delta(alpha)/alpha (alpha = fine-structure constant) --- Patricia Bauer CDS 1993 Nov 10 J_A+AS_104_89.xml uvby-beta photometry of all stars earlier than G0 and brighter than m_pg = 10.3 mag in Selected Area 194 J/A+AS/104/9 J/A+AS/104/9 uvby-beta photometry of all stars earlier than G0 uvby-beta photometry of all stars earlier than G0 and brighter than m_pg = 10.3 mag in Selected Area 194 G A P Franco Astron. Astrophys. Suppl. Ser. 104 9 1994 1994A&AS..104....9F dust, extinction ISM: clouds ISM: individual (Southern Coalsack) surveys Four-colour and H{beta} photometry is introduced for 594 stars earlier than G0 in the Kapteyn's Selected Area 194. The results give V, b-y, m_1_, c_1_, and {beta} on the standard systems, with overall rms errors for one observation of one star of 0.009mag, 0.004mag, 0.006mag, 0.009mag, and 0.009mag, respectively. The data cover an area of about 5deg x 5deg and is intended for an investigation of the distribution of the interstellar medium toward the northern part of the Southern Coalsack and its surroundings. A comparison to earlier results obtained by other authors has shown that the c_1_ indices obtained for the late type stars were underestimated, in average, by 0.020mag. Since such difference may account for an error of little more than 10% in the estimated stellar distances, a correction was applied to the c_1_ index of these stars.
uvby-beta photometry of 594 stars in SA 194 Name Star identification in the Potsdam-Spektral Durchmusterung of the Kapteyn's SA 194 --- HD HD number --- MK Michigan two dimensional classification number=1 Houk N. & Cowley A.P. 1975, Univeresity of Michigan Catalogue of Two-Dimensional Spectrl Types for HD Stars, Univ. of Michigan, Ann Arbor, Vol.1 --- RAh Right Ascension 1900.0 h RAm Right Ascension 1900.0 min RAs Right Ascension 1900.0 s DE- Declination sign --- DEd Declination 1900.0 deg DEm Declination 1900.0 arcmin V computed V magnitude on the Johnson system mag e_V mean error of V 0.001mag n_V When *, the star is probably variable --- (b-y) (b-y) colour index mag e_(b-y) mean error of (b-y) 0.001mag m1 colour indices difference m1 mag e_m1 mean error of m1 0.001mag c1 colour indices difference c1 mag e_c1 mean error of c1 0.001mag o_ubvy Number of observations in uvby --- Hbeta Hbeta index mag e_Hbeta mean error of Hbeta 0.001mag o_Hbeta Number of observations in Hbeta --- Patricia Bauer CDS 1994 Mar 21 J_A+AS_104_9.xml Catalogue of CP stars with references to short time scale variability J/A+AS/105/125 J/A+AS/105/125 Catalogue of CP stars with references to Catalogue of CP stars with references to short time scale variability V P Malanushenko N S Polosukchina W W Weiss Astron. Astrophys. Suppl. Ser. 105 125 1994 1994A&AS..105..125M catalogs stars: chemically peculiar stars: oscillations stars: variables: general A catalogue was compiled which contains all references in the literature since 1962 related to variations of CP stars on time scales shorter than the rotation period. The role of this catalogue lies in the unbiased listing of all available references, and not in a critical evaluation.
Catalogue of variability of CP stars HD HD number --- Name Other name --- Sp Spectral type --- ref. references (in file refs) --- table1.tex LaTex version of table1 Patricia Bauer CDS 1994 Feb 21 J_A+AS_105_125.xml Lyrae stars of Omega Centauri Revisited I. Catalogue of Fourier decomposition parameters J/A+AS/105/145 J/A+AS/105/145 Lyrae stars of Omega Centauri Revisited I. Catal Lyrae stars of Omega Centauri Revisited I. Catalogue of Fourier decomposition parameters J O Petersen Astron. Astrophys. Suppl. Ser. 105 145 1994 1994A&AS..105..145P globular clusters: individual (Omega Cen) stars: oscillations stars: variables: general Mean light curves of 56 RRc and 75 RRab variables in {omega} Cen published by Martin (1938) are used to calculate Fourier decomposition parameters of order N = 5 and 7 and their standard deviations. Besides the Fourier parameters our catalogue contains additional quantities describing the form of light curves. Calculation of the standard deviations is briefly described, and it is shown that these formal errors are also realistic error estimates in typical cases. For 30 stars detailed comparisons between Fourier parameters derived from mean light curves and from the original observations are performed. We find no significant difference between the calculated parameter values in the two types of reduction. This result allows safe use of a large amount of mean light curves published in the literature. A few problems in applications of Fourier parameters are briefly discussed. The physical meaning of the Fourier parameters is not clear. Several representations of the results of Fourier decomposition have been used in the literature. Since we find no convincing argument for preferring one specific representation, we recommend publication of results of Fourier analysis of light curves allowing a wide variety of light curve characteristics to be investigated.
Amlitude ratio and phase differences N Martin's variable number --- P Period d m0 Fourier mean magnitude mag A Fourier amplitude mag H1 Fourier parameter H1 mag/rad Phi1 Fourier parameter Phi1 mag/rad R21 Amplitude ratio R21 --- R31 Amplitude ratio R31 --- R41 Amplitude ratio R41 --- R51 Amplitude ratio R51 --- R61 Amplitude ratio R61 --- R71 Amplitude ratio R71 --- Phi21 Phase difference Phi21 rad Phi31 Phase difference Phi31 rad Phi41 Phase difference Phi41 rad Phi51 Phase difference Phi51 rad Phi61 Phase difference Phi61 rad Phi71 Phase difference Phi71 rad e_R21 std. deviation of amplitude ratio R21 --- e_R31 std. deviation of amplitude ratio R31 --- e_R41 std. deviation of amplitude ratio R41 --- e_R51 std. deviation of amplitude ratio R51 --- e_R61 std. deviation of amplitude ratio R61 --- e_R71 std. deviation of amplitude ratio R71 --- e_Phi21 std. deviation of phase difference Phi21 rad e_Phi31 std. deviation of phase difference Phi31 rad e_Phi41 std. deviation of phase difference Phi41 rad e_Phi51 std. deviation of phase difference Phi51 rad e_Phi61 std. deviation of phase difference Phi61 rad e_Phi71 std. deviation of phase difference Phi71 rad Fourier amplitudes and phases N Martin's variable number --- P Period d m0 Fourier mean magnitude mag A Fourier amplitude mag e_f std deviation on fit mag Np Number of mean point --- H1 Fourier amplitude H1 mag H2 Fourier amplitude H2 mag H3 Fourier amplitude H3 mag H4 Fourier amplitude H4 mag H5 Fourier amplitude H5 mag Phi1 Phase constant Phi1 rad Phi2 Phase constant Phi2 rad Phi3 Phase constant Phi3 rad Phi4 Phase constant Phi4 rad Phi5 Phase constant Phi5 rad f0 Phase of the point of the ascending branch of the curve with m=m0 --- fm Phase at the median magnitude m_m = (m_max + m_min)/2 --- ft Phase at m_t = (2m_max + m_min)/3 --- fmax Phase at light maximum --- fmin Phase at light minimum --- e_H1 std. deviation of H1 mag e_H2 std. deviation of H2 mag e_H3 std. deviation of H3 mag e_H4 std. deviation of H4 mag e_H5 std. deviation of H5 mag e_Phi1 std. deviation of Phi1 rad e_Phi2 std. deviation of Phi2 rad e_Phi3 std. deviation of Phi3 rad e_Phi4 std. deviation of Phi4 rad e_Phi5 std. deviation of Phi5 rad w0 Widths w0 --- wm Widths wm --- wt Widths wt --- Ske Skewneess parameter --- Acu Acuteness parameter --- D Distance from the center (on plate) mm Patricia Bauer CDS 1994 Jan 31 J_A+AS_105_145.xml Proper motions of stars in the region of open cluster NGC 2286 and its membership study J/A+AS/105/15 J/A+AS/105/15 Proper motions of stars in the region of open cluster Proper motions of stars in the region of open cluster NGC 2286 and its membership study K P Tian J -L Zhao F Van Leeuwen Astron. Astrophys. Suppl. Ser. 105 15 1994 1994A&AS..105...15T astrometry open clusters and associations: individual (NGC 2286) Relative proper motions, their corresponding observed errors and membership probabilities of 2400 stars in the open cluster NGC 2286 region are determined from ASTROSCAN measurements of 8 plates made at Leiden Observatory. The plates have the maximum epoch difference of some 70 years and were taken with the double astrograph at Zo-Se station of Shanghai Observatory, which has an aperture of 40 cm, a focal length of 6.9 m and a scale of 30 arcsec/mm. The number of stars with membership probabilities higher than 0.7 and radial distances from the cluster centre less than 12' is 90. The average standard errors of proper motions vary from +/-0.0007"/yr for bright stars in the inner part of the field to some +/-0.0016"/yr for faint stars in the outer part of the field, and are statistically dependent on the number of measured plates per star. It is found from an analysis of the surface number density distribution of cluster members that the angular radius of NGC 2286 is some 12' and the corresponding linear radius 4.5 pc.
Catalogue of proper motion and membership probabilities in the NGC2286 No Ordinal number of stars --- ID Identification numbers in the Li's catalogue --- X X coordinates cm Y Y coordinates cm n_B An * indicates that the photographic magnitude is taken from Chicarini --- B Photographic magnitude mag BL Magnitudes of stars listed in Li's catalogue mag MuX X-proper motion (arcsec/century) 10mas/yr e_MuX Observed error of X-proper motion 10mas/yr MuY Y-proper motion (arcsec/century) 10mas/yr e_MuY Observed error of Y-proper motion 10mas/yr P Proper motion membership probabilities % W Numbers of measured plates of stars --- Patricia Bauer CDS 1994 Jan 19 J_A+AS_105_15.xml New proper-motion stars south of declination -40deg and right ascension between 16h and 24h J/A+AS/105/179 J/A+AS/105/179 New proper-motion stars Dec<-40, 16<RA<24h New proper-motion stars south of declination -40deg and right ascension between 16h and 24h H Woblewski C Torres Astron. Astrophys. Suppl. Ser. 105 179 1994 1994A&AS..105..179W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/78/231 : Dec<-40, 0<RA<4h30, stars 1 to 144 (Wroblewski+ 1989) J/A+AS/91/129 : Dec<-40, 0<RA<4h30, stars 145 to 521 (Wroblewski+ 1991) J/A+AS/115/481 : -30<Dec<-5, 0<RA<9h, stars 1070 to 1563 (Wroblewski+ 1996) J/A+AS/83/317 : LTT stars, Dec<-40, 0<RA<4h30 (Wroblewski+ 1990) J/A+AS/92/449 : LTT stars, Dec<-40, 4h30<RA<16h (Wroblewski+ 1992) J/A+AS/110/27 : LTT stars, Dec<-40, 16<RA<24h (Wroblewski+, 1995) Luyten W.J. 1957, A Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motions Exceeding 0.2 arcsec Annualy (The Lund Press, Minneapolis, Minnesota). Luyten W.J. 1979, LHS Catalogue, University of Minnesota, Minneapolis, Minnesota. (Cat. <I/87>) Proper motions astrometry proper motions Data are given for 548 new proper-motion stars with {mu}>0.15arcsec/year found on 23 areas covering 25 square degrees each. These are located south of declination -40deg and between 16h and 24h in right ascension. Photographic magnitudes range from 10.0 to 20.0. Twenty stars have proper motions larger than 0.5arcsec/year a magnitude range between 14.0 and 19.5
Positions and relative proper motions WT Running number --- Loc Localisation (area and number) --- mpg Photographic magnitude, accurate to 0.5mag mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RAh2000 Right Ascension 2000 (hours) h RAm2000 Right Ascension 2000 (minutes) min RAs2000 Right Ascension 2000 (seconds) s DE-2000 Declination 2000 (sign) --- DEd2000 Declination 2000 (degrees) deg DEm2000 Declination 2000 (minutes) arcmin DEs2000 Declination 2000 (seconds) arcsec pm Total proper motion arcsec/yr e_pm Mean error on pm arcsec/yr pmPA Position angle (North to East) of the proper motion in J2000 equinox deg Remark Remarks number=1 '4' when proper-motion is the mean of #4 pairs of plates (*), '6' when proper-motion is the mean of #6 pairs (**). --- James Marcout, Patricia Bauer CDS 1997 Mar 13 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_105_179.xml The optical identification status of the 1 Jy radio source catalogue J/A+AS/105/211 J/A+AS/105/211 Optical identification status of 1Jy catalogue The optical identification status of the 1 Jy radio source catalogue M Stickel K Meisenheimer H Kuehr Astron. Astrophys. Suppl. Ser. 105 211 1994 1994A&AS..105..211S III/175 : (Optical spectroscopy of 1Jy, S4 and S5 sources) J/A+AS/98/393 : ( ) J/A+AS/103/349 : ( ) J/A+AS/105/67 : (Optical identifications from 1Jy, S4, S5) J/A+AS/105/211 : (Optical identification of 1Jy) J/A+AS/115/11 : (Optical identifications from 1Jy, S4, S5) Cross identifications Radio sources BL Lacertae objects: general catalogs galaxies: general quasars: general radio continuum: galaxies Optical identifications, magnitudes, redshifts, and polarization data have been gathered from an extensive literature search to form an update of the optical data for the radio sources of the 1 Jy catalogue. Of the 527 radio sources in the revised catalogue, 97% have optical counterparts, and redshifts are given for 90% of the optically identified sources. For all but a few sources, accurate interferometer radio position are provided. References are made to well known compilations as well as to individual papers, often supplemented by special notes on individual objects.
Optical data for the 1 Jy radio sources Seq Sequence Number --- Name Object name --- m Magnitude of the optical identification mag Type Type of the optical identification --- l_z limit flag for lower redshift limits --- z redshift of the optical identification --- u_z uncertainty sign for uncertain redshifts --- l_Pol limit flag on Pol --- Pol. "True" optical polarization % n_P Polarization flags v = polarization variable g = polarization contaminated by galaxy light ? = variability uncertain --- e_P error of polarization measurement --- N(P) number of polarization measurements n = more than 10 polarization measurements --- Ref references to polarization measurements and other catalogues number=1 References: B Hewitt & Burbidge (1993) Be Hewitt & Burbidge (1991) C Spinrad et al. (1985) G Burbidge & Crowne (1979)) W Wall & Peacock (1985) V Veron-Cetty & Veron (1991) BH75 Babadzhanyants & Hagen-Thorn (1975) BIEA81 Biermann et al. (1981) BREA86 Brindle et al. (1986) CEA88 Courvoisier et al. (1988) FM88 Fugmann & Meisenheimer (1988) IT88 Impey & Tapia (1988) IT90 Impey & Tapia (1990) IBT82 Impey et al. (1982) ILT91 Impey et al. (1991) ISLX93 Impey et al. (1993) K76 Kinman (1976) KM93 Kock & Meisenheimer (1993) KS90 Kuehr & Schmidt (1990) L90 Luna (1990) MAR80 Marchenko (1980) MMA78 Maza et al. (1978) MEA90 Mead et al. (1990) M79 Maza (1979) MS81 Moore & Stockman (1981) MS84 Moore & Stockman (1984) PEA79 Puschell et al. (1979) PEA83 Puschell et al. (1983) PS80 Puschell & Stein (1980) SMA84 Stockman et al. (1984) SMEA86 Smith et al. (1986) SBEH87 Smith et al. (1987) SSJE93 Smith et al. (1993) ST86 Stahl et al. (1986) STREA72 Strittmatter et al. (1972) V73 Visvanathan (1973) WMSI93 Webb et al. (1993) WWB80 Wills et al. (1980) WWB93 Wills et al. (1993) --- Radio data for the 1 Jy radio sources Seq Sequence number --- Name Object name --- RAh Right ascension 1950 (hours) h RAm Right ascension 1950 (minutes) min RAs Right ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec PosRef Reference to radio position --- S_5GHz 5 GHz flux Jy s(11-6) two-point spectral index between 11 and 6 cm --- RadTyp Type of radio spectrum SS = Steep spectrum FS = Flat spectrum --- FR-class Fanaroff-Riley classification number=1 References: A Waltman et al. (1981) AC White (1992) C Spinrad et al. (1985) CO Condon et al. (1991) D Pearson & Readhead (1988) DS Duncan & Sproats (1992) EK Ekers et al. (1989) F1 White et al. (1987) F2 White et al. (1991) FY Fey et al. (1992) I Bridle et al. (1972) J Kuehr et al. (1981a) JO Jones (1989) L Peacock & Wall (1981) M1 Morabito et al. (1982) M2 Morabito et al. (1983) M3 Morabito et al. 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Phys. 25, 233 Wilkes B.J. 1986, MNRAS 218, 331 Willis A.G., Strom R.G., Wilson A.S. 1974, Nat 250, 625 Willis A.G., Strom R.G. 1978, A&A 62, 375 Wills B.J., Wills, D., Douglas J.N. 1973, AJ 78, 521 Wills D., Wills B.J., Breger M., Hsu J.-C. 1980, AJ 85, 1555 Wills B.J., Wills D., Breger M., Antonucci R.R.J., Barvainis R. 1993, ApJ 398, 454 Wright A.E., Peterson B.A., Jauncey D.L., Condon J.J. 1979, ApJ 229, 73 Wright A.E., Ables J.G., Allen D.A. 1983, MNRAS 205, 793 Wright A., Otrupcek R. 1990, Parkes Catalogue, Australia Telescope National Facility Xu W., Lawrence C.R., Readhead A.C.S., Pearson T.J. 1993, AJ, in press --- NS Number of Sources number= 0008-421 : The empty field classification is due to Prestage & Peacock (1983) and Torres & Wroblewski (1987). 0010+405 : The new classification as a galaxy as well as its redshift is given in Stickel & Kuehr (1993a). The redshift has previously been listed by Biermann et al. (1987), based on spectra taken by one of us (H.K.) with the Steward Observatory 90" telescope. 0019-000 : The identification and magnitude have been taken from Veron & Veron (1975). The optical counterpart has also been classified as a galaxy by McEwan et al. (1975). However, Torres & Wroblewski (1987) find an optical blank field at the radio position, which may indicate that this object is optically variable. A m = 18.4 mag galaxy has been suggested as the optical counterpart by Stanghellini et al. (1993). However, their listed J2000.0 radio position lies about 30' south of that tabulated in the PKS catalogue (Wright & Otrupcek 1990). 0022-423 : A faint optical counterpart of unknown type has been found by Torres & Wroblewski (1987). A B-band CCD image taken with the 2.2m telescope on La Silla, Chile, in October 1986 shows that this object is an unresolved QSO. The optical magnitude is taken from O'Dea et al. (1991). 0022-297 : The identification and magnitude have been taken from Bolton et al. (1965). The optical spectrum and redshift are given in Stickel et al. (1993a) 0023-263 : The identification and magnitude have been taken from Prestage & Peacock (1983). The optical counterpart has also been classified as a galaxy by Saikia et al. (1987). The redshift is given in Tadhunter et al. (1993). 0026+346 : The classification as a galaxy as well as the optical magnitude was derived from an R - band CCD image taken with the 3.5m telescope on Calar Alto, Spain, in September 1989. The image confirms the classification given by Prestage & Peacock (1983), while the classification as a QSO by Rieke et al. (1979) is rejected. 0039-445 : The identification and magnitude have been taken from Savage (1976). The optical counterpart has also been classified as a galaxy by Lue (1974). The redshift is given in Tadhunter et al. (1993). 0040+517 : The redshift has been taken from Lawrence et al. (1986). The redshift listed by Spinrad et al. (1985) and Wall & Peacock (1985) is incorrect. 0042-357 : No identification has been found in the literature. 0043-424 : The identification, magnitude and redshift have been taken from Whiteoak (1972). A different redshift is given in Tadhunter et al. (1993). 0056-572 : The identification as a QSO is due to Bolton & Savage (1977) and White et al. (1991). The optical magnitude has been taken from White et al. (1991). 0105-163 : The classification as a galaxy is due to Prestage & Peacock (1983) and Moseley et al. (1970). The redshift is given by Tadhunter et al. (1993). 0108+388 : The identification and optical magnitude have been taken from O'Dea et al. (1991). The redshift has been made available to us by C. Lawrence (1993, priv. comm.). 0112-017 : The redshift of z = 1.381 has been taken from Baldwin et al. (1989). 0113-118 : The identification and magnitude have been taken from Wright et al. (1983). The uncertain redshift given by Wright et al. (1983) has been confirmed with spectra taken by one us (H.K.) with the Steward Observatory 90" telescope and the Multiple Mirror Telescope. 0114-211 : The classification as an empty field is due to Bozyan (1979), Prestage & Peacock (1983) and Ekers et al.(1989). 0117-155 : The identification and magnitude have been taken from Fugmann et al. (1988). The optical counterpart has also been classified as galaxy by Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). 0118-272 : The optical spectrum and the absorption line redshift are given in Falomo (1991) and Stickel et al. (1993b). An incorrect absorption line redshift is listed in Veron-Cetty & Veron (1991). 0131-522 : The classification of the optical counterpart as a QSO is due to Savage et al. (1976), Peterson et al. (1976) and White et al. (1991). The optical magnitude has been taken from White et al. (1991). 0138-097 : The optical spectrum and the absorption line redshift are given in Stickel et al. (1993b). 0149+218 : The radio spectral index has been taken from the Parkes catalogue (Wright & Otrupcek 1990). 0157-311 : The optical magnitude has been taken from Prestage & Peacock (1983). The redshift has been made available to us by J. A. Peacock (1993, priv. comm.). 0201-440 : This radio source has tentatively been identified with a m = 19 mag QSO by Fugmann et al. (1988). 0202+149 : The identification and magnitude were taken from Fugmann & Meisenheimer (1988). 0218+357 : The redshift of the intervening absorption line system has been measured by Browne et al. (1993) and Stickel & Kuehr (1993b). The optical magnitude is given in Stickel & Kuehr (1993b). This source is most likely a gravitational lens system (O'Dea et al. 1992a, Patnaik et al. 1993, Browne et al. 1993). 0221+067 : This source is probably optically variable, since White et al. (1988) give m = 19 mag, while Fugmann & Meisenheimer (1988) list m = 16.7 mag. 0223+341 : The identification and magnitude have been taken from Peacock et al. (1981). 0235-197 : The identification and magnitude were taken from Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). 0235+164 : The optical magnitude has been taken from Argue et al. (1973). The magnitude listed in the catalogues of Hewitt & Burbidge (1993) and Veron-Cetty & Veron (1991) refers to an optical outburst. 0252-712 : The identification and magnitude have been taken from Savage et al. (1977). The redshift is given by Tadhunter et al. (1993). 0302-623 : The identification and magnitude have been taken from Wall & Cannon (1973). 0308-611 : The identification and magnitude have been taken from White et al. (1991). 0316+162 : The identification and magnitude have been taken from Fugmann et al. (1988). The radio source has also been identified by Stanghellini et al. (1993). 0319+121 : The optical magnitude has been taken from Bolton & Ekers (1967). The redshift has been derived from several spectra taken by one of us (H.K.) with the Steward Observatory 90" telescope and the Multiple Mirror Telescope. The redshift is also listed in Spencer et al. (1989). 0332+078 : The identification and magnitude were taken from Fugmann & Meisenheimer (1988). 0347+057 : The identification and magnitude have been taken from Fugmann et al. (1988). The redshift is given by Allington-Smith et al. (1991). 0400-319 : The classification as an empty field is due to Saikia et al. (1987). 0402+379 : The identification and magnitude were taken from Wills et al. (1973). The optical spectrum and redshift are given in Stickel et al. (1993a). 0403+768 : The identification and magnitude have been taken from Peacock et al. (1981). The galaxy, which lies midway between the radio lobes, has also been detected on an R - band CCD image taken with the 2.2m telescope on Calar Alto, Spain. The redshift is given in O'Dea et al. (1991) 0407-658 : The radio source has tentatively been identified with a 18 mag QSO by Hunstead (1971) and Prestage & Peacock (1983). 0409-752 : The identification, optical magnitude, and redshift have been taken from Alvarez et al. (1993). The redshift has also been given by Tadhunter et al. (1993). 0426-380 : The absorption line redshift given in Stickel et al. (1991,1993b) is incorrectly listed as emission line redshift in the catalogue of Hewitt & Burbidge (1993). 0427-539 : The identification, magnitude, and redshift were taken from Danziger & Goss (1983). The redshift is also given by Tadhunter et al. (1993) 0437-454 : The identification and magnitude have been taken from Jauncey et al. (1989). 0442-282 : The identification and magnitude have been taken from Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). 0446+112 : The radio source has been identified with a galaxy by Hoskins et al. (1974). This identification was confirmed with a CCD image taken with the 2.2m telescope on La Silla, Chile, in October 1986, from which the R - band magnitude of m = 20.6 mag was derived. 0453-301 : The identification and magnitude were taken from Shimmins & Bolton (1974). 0454+844 : The redshift of z = 0.112 has been made available to us by C. Lawrence (1993, priv. comm.). This value is in obvious contrast to the lower limit of z > 0.2 suggested in Stickel et al. (1993b) on the basis of the unresolved appearance on the direct image. This indicates that the host galaxy of this BL Lac object has an unusually low optical luminosity (see the discussion in Stickel et al. 1993b). 0500+019 : The identification and magnitude were taken from Fugmann et al. (1988). The same optical counterpart has also been found by Torres & Wroblewski (1987) and was described as very faint and of unknown type. 0511-305 : The identification and magnitude were taken from Bolton et al. (1965). 0514-459 : The identification and magnitude have been taken from Bolton & Savage (1977). The optical spectrum and redshift are given in Stickel et al. (1993a). 0521-365 : An incorrect redshift is listed in Burbidge & Crowne (1979), Wall & Peacock (1985), Burbidge & Hewitt (1987), and Hewitt & Burbidge (1987,1991,1993). The correct redshift is given by Ulrich (1981), Falomo et al. (1989), and Stickel et al. (1993a). 0524-460 : The identification and magnitude were taken from Jauncey et al. (1989). The optical spectrum and redshift is given in Stickel et al. (1993a). 0528+134 : The identification and magnitude have been taken from Fugmann & Meisenheimer (1988). The redshift has been derived from spectra taken by one of us (H.K.) with the Steward Observatory 90" telescope and the Multiple Mirror Telescope. The identification and redshift were also given by Stanghellini et al. (1993). 0539-057 : The identification and magnitude were taken from Fugmann & Meisenheimer (1988). The optical spectrum and redshift are given in Stickel & Kuehr (1993b). The incorrect redshift given by Chu et al. (1986) is also listed in the catalogue of Veron-Cetty and Veron (1991). 0602+673 : The identification and optical magnitude have been taken from Meisenheimer & Roeser (1983). 0605-085 : The redshift has also been listed by Allington-Smith et al. (1991) and Stickel et al. (1993a). 0615+820 : The redshift listed by Eckart et al. (1986) is based on spectra taken by one of us (H.K.) with the Steward Observatory 90" telescope and the Multiple Mirror Telescope. 0625-536 : The identification, optical magnitude, and redshift have been taken from Danziger & Goss (1983). The redshift is also given by Tadhunter et al. (1993). 0625-354 : The identification and magnitude have been taken from Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). 0646-306 : The unresolved optical counterpart of this radio source is probably variable, since Saikia et al. (1987) find m = 21 mag while Fugmann et al. (1988) give m = 18.6 mag. The lower limit of the optical polarization is based on a measurement with only a single analyzer position angle (see Fugmann & Meisenheimer 1988). 0707+476 : The identification and magnitude were taken from Meisenheimer & Roeser (1983). The redshift has been derived from a spectrum taken by one of us (H.K.) with the Steward Observatory 90" telescope. No entry for the optical polarization is given in Table 2, since the object measured by Wills et al. (1993) is a foreground star (see Meisenheimer & Roeser 1983). 0710+439 : The identification and optical magnitude have been taken from Stanghellini et al. (1993). The redshift is listed in Pearson & Readhead (1988). 0742+103 : The faint identification proposed by Fugmann et al. (1988) has not been detected on R - and I - band CCD images taken with the 2.2m telescope on La Silla, Chile, in March 1985 and the 2.2m telecope on Calar Alto, Spain, in December 1985. The radio source is thus classified as an empty field, which also disagrees with O'Dea et al. (1991). 0743-673 : The redshift of z = 1.511 has been taken from Espey et al. (1989). This value has also been given by Jauncey et al. (1989). The redshift listed by Wall & Peacock (1985), Hewitt & Burbidge (1989), and Veron-Cetty & Veron (1991) is incorrect. 0806-103 : The identification, magnitude, and redshift have been taken from Tabara & Inoue (1980), who refer to Gardner et al. (1969). The redshift has also been listed by Tadhunter et al. (1993). 0820+225 : The emission lines and the absorption line redshift listed in Hewitt & Burbidge (1993) are obviously typographical errors. The optical spectrum and redshift is given in Stickel et al. (1993b) 0825-202 : The identification and magnitude were taken from Bolton & Kinman (1966). The optical spectrum and redshift is given in Stickel et al. (1993a). 0828+493 : The optical spectrum and redshift is given in Stickel et al. (1993b) 0834-196 : The uncertain type and magnitude of the optical counterpart is based on a tentative identification by Fugmann et al. (1988). 0836+710 : The optical spectrum and redshift is given in Stickel & Kuehr (1993a). The redshift has previously been listed by Eckart et al. (1986), based on spectra taken by one of us (H.K.) with the Steward Observatory 90" telescope and the Multiple Mirror Telescope. 0839+187 : The redshifted listed in Veron-Cetty & Veron (1991) is incorrect. 0858-279 : The identification and magnitude were taken from Prestage & Peacock (1983). The optical spectrum and redshift is given in Stickel et al. (1993b). An incorrect redshift has been given by Thompson et al. (1991) and is listed in the catalogues of Veron-Cetty & Veron (1991) and Hewitt & Burbidge (1993). 0859-257 : The identification and magnitude have been taken from Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). 0915-118 : The redshift listed in Burbidge & Crowne (1979) is incorrect. 0917+624 : The optical spectrum and the redshift is given in Stickel & Kuehr (1993b). The redshift previously listed by Quirrenbach et al. (1989) and Qian et al. (1991) was derived from a spectrum taken by one of us (H.K.) with the Mount Palomar 5m telescope. 0941-080 : The identification and optical magnitude have been taken from Stanghellini et al. (1993). 0945+664 : The identification and magnitude were taken from Peacock et al. (1981). 0947+145 : The identification, magnitude and redshift have been taken from Spinrad et al. (1985) 1005+077 : The identification, magnitude and redshift have been taken from Spinrad et al. (1985) 1015-314 : The identification and magnitude were taken from Prestage & Peacock (1983). 1031+567 : The identification and optical magnitude have been taken from Stanghellini et al. (1993). The redshift is listed in Dunlop et al. (1989). 1039+029 : McEwan et al. (1975) and Veron & Veron (1977) find an optical blank field at the radio position. 1039+811 : The redshift is derived from spectra taken by one of us (H.K.) with Steward Observatory 90" telescope and has previously been listed by Eckart et al. (1986). 1057-797 : The identification and magnitude have been taken from Jauncey et al. (1989). 1117+146 : The identification and magnitude were taken from Wills et al. (1973). 1143-483 : The identification and magnitude were taken from Hunstead (1971). 1150+812 : The redshift is derived from spectra taken by one of us (H.K.) with Steward Observatory 90" telescope and has previously been listed by Eckart et al. (1986). 1157+732 : The redshift has been taken from McCarthy (1988). 1203+645 : The redshift listed by Herbig & Readhead (1992) is incorrect. 1213-172 : This radio source lies close to the 2.6 mag star gamma Corvus. A direct CCD image taken with the 3.5m telescope on Calar Alto, Spain, in June 1993 shows a m = 21.4 mag resolved galaxy at the radio position. 1216+487 : The optical spectrum and redshift is given in Stickel & Kuehr (1993c). 1221-423 : The identification and magnitude have been taken from Lue (1970). The redshift is given by Simpson et al. (1993). 1245-197 : The identification, magnitude, and redshift were taken from O'Dea et al. (1991). 1246-410 : The identification, magnitude, and redshift have been taken from Burbidge & Burbidge (1972). 1306-095 : The identification and magnitude have been taken from Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). 1308-220 : The classification as an optical blank field is due to Torres & Wroblewski (1987). A possible candidate for the optical counterpart has been proposed by Prestage & Peacock (1983). 1313-333 : The redshift is based on two emission lines at lambda = 4232 A and lambda = 6166 A detected by Jauncey et al. (1982) and identified with C III] 1909 and Mg II 2798 at z = 1.210, as described in their notes on individual objects. The incorrect redshift listed in Table II of Jauncey et al. (1982) is obviously a misprint, which also appears in the catalogue of Veron-Cetty & Veron (1991). 1320-446 : The identification and magnitude were taken from Torres & Wroblewski (1986). 1323+321 : The identification and magnitude have been taken from Grueff & Vigotti (1972). The redshift is given in Dunlop et al. (1989). The radio source has also been identified by Stanghellini et al. (1993). 1333-337 : The lobes of the radio source 1333-337 (IC 4296, Killeen et al. 1986), which had previously been listed as the individual sources 1332-33 and 1334-33 (Kuehr et al. 1981a), have been removed from the 1 Jy catalogue. 1334-127 : The uncertain redshift listed in Hewitt & Burbidge (1993) has been confirmed by Stickel et al. (1993a). 1413+349 : The classification as an optical blank field is due Peacock et al. (1981), Meisenheimer & Roeser (1983) and Stanghellini et al. (1993). A possible IR counterpart has been detected by O'Dea et al. (1992b). 1418+546 : The optical spectrum and redshift is given in Stickel et al. (1993b) 1434+036 : The classification as an optical blank field is due to McEwan et al. (1975). 1435+638 : The optical magnitude has been taken from Porcas et al. (1980). 1502+106 : The redshift has been taken from Wright et al. (1979) and Wilkes (1986). The redshift listed in the catalogues of Hewitt & Burbidge (1993) and Veron-Cetty & Veron (1991) is based on a different identification of the spectral features observed by Smith et al. (1977). 1504+377 : The revised classification as a galaxy as well as the optical magnitude and redshift are given in Stickel & Kuehr (1993c). 1518+046 : The identification and magnitude have been taken from Biretta et al. (1985). 1519-273 : The classification as a BL Lac Object as well as the optical spectrum is given by Stickel et al. (1993b) and Veron-Cetty & Veron (1993). 1538+149 : The optical spectrum and redshift is given by Stickel et al. (1993b) 1541-828 : No optical identification has been found in the literature. 1547-795 : The identification and magnitude have been taken from Hunstead (1971) and Shimmins & Bolton (1972). The redshift is given by Tadhunter et al. (1993). 1549-790 : The identification and magnitude were taken from White et al. (1987) and Jauncey et al. (1989). The redshift is given in Veron et al. (1990) and Tadhunter et al. (1993). 1600+335 : Stanghellini et al. (1993) suggested a very faint, possibly extended object as the optical counterpart. A deep R band image taken in June 1993 with the 3.5m telescope on Calar Alto, Spain, confirmed the presence of the optical counterpart and showed it to be a highly elongated or even morphologically disturbed m(R) = 23 mag galaxy. 1602-093 : No optical identification has been found in the literature. 1606+106 : The identification and magnitude have been taken from Bolton et al. (1968). The optical spectrum and redshift is given in Stickel & Kuehr (1993c). A preliminary value for the redshift has been given in Biermann et al. (1987), which was based on spectroscopic observations by one of us (H.K.) with the Steward Observatory 90" telescope. 1607+268 : The identification and magnitude were taken from Biretta et al. (1985). The redshift is listed in Phillips & Shaffer (1983) and O'Dea et al. (1991). The radio source has also been identified by Stanghellini et al. (1993). 1622-297 : The identification and optical magnitude have been taken from Saikia et al. (1987). The redshift has been taken from the PKS catalogue (Wright & Otrupcek 1990). 1622-253 : No optical counterpart has been found by Prestage & Peacock (1983), who marked a nearby object on their finding chart. Saikia et al. (1987) described the field as obscured. A direct CCD image taken with the 2.2m telescope on La Silla, Chile, in March 1985 shows a m = 20.3 mag unresolved object at the radio position given by Prestage & Peacock (1983), which is proposed as the optical counterpart. The optical polarization measured by Impey & Tapia (1990) probably refers to the nearby object of Prestage & Peacock (1983). 1637-771 : The redshift of z = 0.0427 has been taken from Simpson et al. (1993), which is in agreement with the value given by Whiteoak (1972), Burbidge & Burbidge (1972) and Tadhunter et al. (1993). The redshift listed by Danziger & Goss (1983) is incorrect, as has already been noted by Simpson et al. (1993). 1638+124 : The identification and optical magnitude is based on a direct R - band CCD image taken with the 3.5m telescope on Calar Alto, Spain, in June 1991. 1648+015 : The identification and optical magnitude is based on direct R-band CCD images taken with the 3.5m and 2.2m telescopes on Calar Alto, Spain, in June 1992. 1655-776 : The redshift has been taken from Simpson et al. (1993). The redshift listed in Burbidge & Crowne (1979) is incorrect. 1721-026 : The identification of this radio source with m = 15 mag galaxy by Veron (1971) is uncertain (Stickel et al. 1993a). The optical spectrum and redshift of this tentative optical counterpart is given in Stickel et al. (1993a). 1737-608 : The identification and magnitude have been taken from Jones & McAdam (1992). 1740-517 : An uncertain identification with a m = 20.2 mag galaxy has been given by Prestage & Peacock (1983). 1815-553 : The identification and magnitude were taken from White et al. (1991). 1829-718 : No optical identification has been found in the literature. 1829+290 : The identification, the optical magnitude and the redshift is given in Stickel & Kuehr (1993b). The identification and redshift listed by Spencer et al. (1989) is rejected. 1839-486 : The identification and magnitude have been taken from Bajaja (1970). The redshift is given by Tadhunter et al. (1993) and Simpson et al. (1993). 1928+738 : An incorrect redshift is listed in Wall & Peacock (1985). The correct redshift is given in Lawrence et al. (1986) and Stickel et al. (1993a). 1929-397 : The identification and magnitude have been taken from Bolton & Shimmins (1973). The redshift is given by Simpson et al. (1993). 1932-464 : The identification and magnitude have been taken from Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). 1936-623 : The identification and magnitude have been taken from White et al. (1991). 1938-155 : The identification and magnitude have been taken from Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). 1954-552 : The identification and optical magnitude have been taken from Whiteoak (1972). The redshift given by Tadhunter et al. (1993) and Simpson et al. (1993) confirm the uncertain value listed by Whiteoak (1972). 2008-068 : The identification and magnitude were taken from Fugmann et al. (1988). The radio source has also been identified by O'Dea et al. (1990) and Stanghellini et al. (1993). 2020-575 : The identification, magnitude, and redshift were taken from Jones & McAdam (1992). 2029+121 : The classification, optical magnitude, and a tentative redshift are given in Stickel & Kuehr (1993a). 2032-350 : The identification and magnitude were taken from Prestage & Peacock (1983). 2052-474 : The identification, magnitude, and redshift were taken from Murdoch et al. (1984). 2053-201 : The identification and magnitude have been taken from Hazard (1972). The optical spectrum and redshift is given in Stickel & Kuehr (1993c). 2104+763 : The identification, optical magnitude, and redshift have been taken from Smith et al. (1976). 2113+293 : The optical magnitude has been taken from Kuehr (1980). The spectrum and redshift is given in Stickel et al. (1993a). 2128+048 : The extremely faint optical counterpart has been found by Biretta et al. (1985). The redshift has been made available to us by H. Spinrad (1993, priv. comm.). 2135-209 : The identification and magnitude were taken from Prestage & Peacock (1983). The redshift is given by Tadhunter et al. (1993). However, the radio source has been classified as an empty field by Saikia et al. (1987). 2140-816 : No optical identification has been found in the literature. 2149-287 : No optical identification has been found in the literature. 2149+056 : The identification and optical magnitude were taken from O'Dea et al. (1991). The optical spectrum and redshift is given in Stickel & Kuehr (1993a). 2150-520 : This radio source has tentatively been identified with a m = 18 mag QSO by Prestage & Peacock (1983). 2150+173 : The identification and magnitude as well as the featureless optical spectrum are given in Stickel et al. (1993a). 2210+016 : This radio source has tentatively been identified with a m = 21.7 mag QSO by Fugmann et al. (1988). 2245-328 : The redshift has been taken from Jauncey et al. (1982) 2250-412 : The identification and optical magnitude have been taken from Hunstead (1971). The redshift is given by Tadhunter et al. (1993). 2252-530 : A faint object near the plate limit has been proposed as the optical counterpart by Lasker & Smith (1974). The galaxy suggested by Lue (1974) has been discarded by Jones & McAdam (1992). 2255+416 : The identification and magnitude were taken from Fugmann & Meisenheimer (1988). The optical spectrum and the redshift is given in Stickel & Kuehr (1993a,c). The spectral features described therein are in contrast to those listed by Xu et al. (1993), who suggested a redshift of z = 1.724. 2311-452 : An incorrect designation and position for this source is listed in Hewitt & Burbidge (1993). 2317-277 : The identification and magnitude were taken from Bolton et al. (1965). 2319+272 : The optical counterpart of this radio source is a quasar at z = 1.253, which lies behind the cluster Abell 2584. A detailed discussion of this remarkable object can be found in Stickel & Kuehr (1992). 2323-407 : The identification and magnitude has been taken from Lue (1970). 2323+435 : The identification and magnitude were taken from Edwards et al. (1975). The optical spectrum and redshift is given in Stickel et al. (1993a). 2324-023 : The identification and magnitude have been taken from Bolton & Ekers (1966). The optical spectrum and redshift is given in Stickel et al. (1993a). 2324+405 : The identification and magnitude were taken from Cohen et al. (1977). The optical spectrum and the redshift is given by Stickel & Kuehr (1993b). 2331-417 : The identification and magnitude have been taken from Savage et al. (1976). 2333-528 : The classification as an empty field is due to Jauncey et al. (1989). The optical identification proposed by Bolton & Savage (1977) and White et al. (1991) has been discarded by Jauncey et al. (1989) on the basis of an accurate VLBI radio position. 2337-334 : A tentative identification with a very faint object of unknown type has been proposed by Torres & Wroblewski (1987). 2351+456 : The optical spectrum and redshift is given by Stickel & Kuehr (1993b). 0114-476 : The radio flux and the radio spectral index have been taken from Saripalli et al. (1986) and Danziger & Goss (1983), respectively. 0319-453 : The radio and optical properties have been taken from Jones (1989). 0344-345 : The radio flux and the radio spectral index (measured between 408 MHz and 5 GHz) have been taken from Wall & Schilizzi (1979). 0511-484 : The radio flux and the radio spectral index (measured between 408 MHz and 5 GHz) have been taken from Wall & Schilizzi (1979). 0744+559 : The radio flux and the radio spectral index have been taken Saripalli et al. (1986) and Willis et al. (1974), respectively. 1331-098 : The radio flux and the radio spectral index (measured between 408 MHz and 5 GHz) have been taken from Wall & Schilizzi (1979). 1448+634 : The radio flux and the radio spectral index have been taken from Condon et al. (1991). 1514+072 : The radio flux and the radio spectral index have been taken from Condon et al. (1991). 1549+202 : The radio flux and the radio spectral index have been taken Saripalli et al. (1986) and Willis & Strom (1978), respectively. 1557+708 : The radio flux and the radio spectral index have been taken from Condon et al. (1991). The redshift is given by Herbig & Readhead (1992) and Stickel et al. (1993a). 1637+826 : The radio flux and the radio spectral index have been taken from Saripalli et al. (1986) and Wagget et al. (1977), respectively. 2212+135 : The radio flux and the radio spectral index have been taken from Condon et al. (1991). --- Francois Ochsenbein CDS 1994 Feb 17 Manfred Stickel J_A+AS_105_211.xml Stark broadening of Be I spectral lines J/A+AS/105/243 J/A+AS/105/243 Stark broadening of BeI lines Stark broadening of Be I spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 105 243 1994 1994A&AS..105..243D VI/82 : Stark broadening of H lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar MgI lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines Atomic physics atomic data line: profiles molecular data Using a semiclassical approach, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for 28 BeI multiplets. The resulting data have been compared with existing theoretical values.
Stark broadening parameters due to e-, p- and He II-impacts for Be I N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K We FWHM for electron impacts number=2 FWHM denotes the Full Width at Half Maximum 0.1nm de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe+ (4) --- WHe+ FWHM for He II-impacts (2) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dHe+ (4) --- dHe+ shift for He II-impacts (3) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm Sylvie Sahal-Brechot Meudon Patricia Bauer CDS 1994 Feb 17 J_A+AS_105_243.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest. XI: Al XI and Si XII J/A+AS/105/245 J/A+AS/105/245 Stark broadening Al XI and Si XII Stark broadening of spectral lines of multicharged ions of astrophysical interest. XI: Al XI and Si XII M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 105 245 1994 1994A&AS..105..245D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar MgI lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles Using a semiclassical approach, we have calculated electron-, proton-, and HeIII -impact line widths and shifts for 7 AlXI and 9 SiXII multiplets. The results obtained have been used for the study of the behavior of Stark broadening parameters within an isoelectronic sequence.
Stark broadening parameters due to e-, p- and He III-impacts for Al XI and Si XII N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K We FWHM for electron impacts number=2 FWHM denotes the Full Width at Half Maximum 0.1nm de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ (4) --- WHe++ FWHM for He III-impacts (2) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dHe++ (4) --- dHe++ shift for He III-impacts (3) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm Sylvie Sahal-Brechot Meudon Patricia Bauer CDS 1994 Feb 17 J_A+AS_105_245.xml Evolutionary sequences of stellar models with new radiative opacities. IV. Z = 0.004 and Z=0.008 J/A+AS/105/29 J/A+AS/105/29 Evolutionary sequences IV. Evolutionary sequences of stellar models with new radiative opacities. IV. Z = 0.004 and Z=0.008 F Fagotto A Bressan G Bertelli C Chiosi Astron. Astrophys. Suppl. Ser. 105 29 1994 1994A&AS..105...29F stars: evolution stars: interiors We present detailed tabulations of two large grids of stellar models with the initial chemical compositions [Y=0.240, Z=0.004] and [Y=0.250, Z=0.008], computed with the most recent radiative opacities (OPAL) by Iglesias et al. (1992). This paper continues the series initiated by Bressan et al. (1993) for the grid with [Y=0.280, Z=0.020], the reference solar like abundances, followed by Fagotto et al. (1994a) for the grids with compositions [Y=0.230, Z=0.0004] and [Y=0.352, Z=0.05]. The tracks span a wide range of initial masses from 0.6M_{sun}_ to 120M_{sun}_ and extend from the zero age main sequence (ZAMS) till very advanced evolutionary phases. Specifically, low- and intermediate-mass stars are followed till the beginning of the thermally pulsing regime of the asymptotic giant branch phase (TP-AGB), while massive stars are followed till the core C-ignition. The models of low- and intermediate-mass stars are calculated at constant mass, whereas those of massive stars are followed in presence of mass loss by stellar wind incorporating a suitable dependence on the metallicity. The results for all the models are given in extensive tables which summarize also the lifetimes of the various phases and the variations of the surface abundances by dredge-up phenomena and mass loss by stellar wind. The salient features brought by the different metallicity and helium content are briefly outlined. In virtue of their large coverage of masses, evolutionary phases, and chemical compositions, such grids of evolutionary tracks are basic to studies of population synthesis. In particular they are suited to interpret the CMDs of metal-rich globular clusters and of the typical stellar content of the Large Magellanic Cloud.
Evolutionary sequences of low mass stars up to the tip of the RGB. 0.6 < M < 1.8 for z=0.004 Evolutionary sequences of low mass stars up to the tip of the RGB. 0.6 < M < 1.8 for z=0.008 Evolutionary sequences of low mass stars during the core-helium burning and EAGB phases. 0.5 < M < 1.8 for z=0.004 Evolutionary sequences of low mass stars during the core-helium burning and the EAGB phases. 0.5 < M < 1.8 for z=0.008 Evolutionary sequences of intermediate stars up to the TPAGB or carbon-ignition. 1.9 < M < 9.0 for z=0.004 Evolutionary sequences of intermediate stars up to the TPAGB or carbon-ignition. 2.0 < M < 9.0 for z=0.008 m Initial mass Sun Age Age of models yr log(L) Total luminosity Sun log(Teff) Effective temperature K log(G) Surface gravity cm/s2 log(Tc) Central temperature K log(rho_c) Central density g/cm3 COMP Central abundance (by mass) of hydrogen or helium --- X_C Central abundance of 12C --- X_O Central abundance of 16O --- Conv Fractionary mass of the convective core (inclusive of overshoot) --- Q_disc Fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log(L_H) Hydrogen luminosity Sun Q1_H Fractionary mass of the inner border of the hydrogen rich region --- Q2_H Fractionary mass of the outer border of the H-burning region. The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- log(L_He) Helium luminosity Sun Q1_He Fractionary mass of the inner border of the He-burning region (when greater than zero He-burning is in a shell). The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- Q2_He Fractionary mass of the upper border of the He-burning region. The boundary is taken as above. --- log(L_C) Carbon luminosity Sun log(L_nu) Neutrinos luminosity (absolute value) Sun Q_Tmax Fractionary mass of the point where the temperature attains the maximum value --- Evolutionary sequences for massive stars. 12 < M < 120 for z=0.004 Evolutionary sequences for massive stars. 12 < M < 120 for z=0.008 m Initial mass Sun Age Age of models yr M Current value of the mass Sun log(L) Total luminosity Sun log(Teff) Effective temperature K log(G) Surface gravity cm/s2 log(Tc) Central temperature K log(rho_c) Central density g/cm3 COMP Central abundance of hydrogen or helium by mass --- X_C Central abundance of 12C --- X_O Central abundance of 16O --- Conv Fractionary mass of the convective core (inclusive of overshoot) --- Q_disc Fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log(L_H) Hydrogen luminosity Sun Q1_H Fractionary mass of the inner border of the hydrogen rich region --- log(L_He) Helium luminosity Sun log(M_dot) Absolute value of the mass loss rate Sun/yr X_sur Surface abundance by mass of 1H --- Y_sur Surface abundance by mass of 4He --- XC_sur Surface abundance by mass of 12C --- XN_sur Surface abundance by mass of 14N --- XO_sur Surface abundance by mass of 16O --- table1.tex Latex version of table1(a,b) table2.tex Latex version of table2(a,b) table3.tex Latex version of table3(a,b) table4.tex Latex version of table4(a,b) Patricia Bauer CDS 1994 Jan 21 J_A+AS_105_29.xml High-dispersion microfiche atlas of OB stars for the first 10 years of IUE J/A+AS/105/305 J/A+AS/105/305 High-dispersion microfiche atlas of OB stars for High-dispersion microfiche atlas of OB stars for the first 10 years of IUE R C Bohlin H F Henrichs J S Nichols Astron. Astrophys. Suppl. Ser. 105 305 1994 1994A&AS..105..305B atlases catalogs stars: early-type ultraviolet: stars An atlas on microfiche is described containing nearly 7000 high-dispersion spectra of OB stars obtained during the first 10 years with the IUE satellite. The data set is nearly complete for the selected time interval. The plotted wavelength range is from 1160 to 1890 A at the original IUE sampling intervals.
Catalog of spectra included in the High-dispersion microfiche atlas of OB stars NF Microfiche number --- Name Object name --- Pro Program identification --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec V Visual magnitude mag E When E, the following value is E(B-V) --- B-V B-V or E(B-V) mag Sp Spectral type --- Ob Object class number=1 Classification of objects 07 Interplanetary medium 26 BE 12 Main Sequence O 27 Bp 13 Supergiant O 28 SDB 14 OE 30 A0-A3 V-IV 15 OF 39 Composite 16 SD O 52 Irregular Variables 20 B0-B2 V-IV 53 Regular Variables 21 B3-B5 V-IV 59 X-Ray 22 B6-B9,5 V-IV 60 Shell Star 23 B0-B2 III-I 66 Interacting Binaries 24 B3-B5 III-I 99 Nulls and Flat Fields (NASA Log) 25 B6-B9.5 III-I --- SWP SWP (Short Wavelength Prime Camera) number --- A Aperture, L for large (10 x 20 arcsec) S for small (3 arcsec ) T for trailed images M for multiple exposures --- L Status of large aperture (O: open, C: close) --- EXPm Exposure time (minutes) min EXPs Exposure time (seconds) s OBSy Observation date (year) yr OBSd Observation date (day) d OBSh Observation date (hours) h OBSm Observation date (minutes) min S Station, V for VILPA G for Goddard SFC --- PROCy Processing date (year) h PROCd Processing date (day) d R Observer's comments --- Patricia Bauer CDS 1994 Jan 31 UNKNOWN UNKNOWN For more explanations, see any ESA IUE Newsletter. J_A+AS_105_305.xml On the spectra and photometry of M-giant stars J/A+AS/105/311 J/A+AS/105/311 On the spectra and photometry of M-giant stars On the spectra and photometry of M-giant stars M A Fluks B Plez P S The D De Winter B E Westerlund H C Steenman Astron. Astrophys. Suppl. Ser. 105 311 1994 1994A&AS..105..311F stars: late-type stars: giants stars: fundamental parameters ISM: extinction From a sample of 97 very bright M-giant stars in the Solar neighbourhood, high-quality `intrinsic' spectra in the spectral range [380-900]nm for all M-spectral subclasses of the Case and MK classification systems are obtained. The results are fitted to photospheric synthetic spectra in the range [99-12500]nm in order to infer the corresponding continua. The synthetic spectra are also compared to the intrinsic spectra. The effective temperatures are derived and mathematical spectral classification criteria are found. The (UB)j(VRI)c(JHKLM)eso photometric data of the sample are also given.
Spectral + Astrometric data of programme stars Double Flag indicating a double system (from HIC) --- Nr Running number --- GC GC identification --- HD HD identification --- HIC HIC (Hipparcos Input Catalogue) identification --- HR HR = Bright Star identification --- n_SAO SAO differs in Bright Star Catalogue --- SAO SAO identification --- Sp Spectral type from HR --- Cover [0:7] Spectral Coverage number=1 1 = IUE(UV) 2 = IDS(visual) 3 = CCD(visual) 4 = CCD(near-infrared) 5 = IRAS(IR) 6 = (UB)j(VRI)c 7 = (JHKLM)eso --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s pmRA Proper motion in RA s/yr DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec pmDE Proper motion in DE arcsec/yr plx Parallax arcsec RV Radial velocity km/s Photometric data Nr Running number --- U U magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag B B magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag V V magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag R R magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag I I magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag Date1 Calendar date (MM/DD/YYYY) for UBVRI --- JD1 Julian date for UBVRI observations d J J magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag H H magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag K K magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag L L magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag M M magnitude number=2 Photometric magnitudes are described in Menzies et al. (1980). mag Date2 Calendar date (MM/DD/YYYY) for JHKLM --- JD2 Julian date for JHKLM observations d Statistical extinction Nr Running number --- GLON Galactic longitude deg GLAT Galactic latitude deg r Distance pc Sp Spectral class --- E(B-V) Color excess mag a(U) Absorption in U band for the spectral class mag a(B) Absorption in B band for the spectral class mag a(V) Absorption in V band for the spectral class mag a(R) Absorption in R band for the spectral class mag a(I) Absorption in I band for the spectral class mag a(J) Absorption in J band for the spectral class mag a(H) Absorption in H band for the spectral class mag a(K) Absorption in K band for the spectral class mag a(L) Absorption in L band for the spectral class mag a(M) Absorption in M band for the spectral class mag Extinction law up to 250um lambda Wavelength nm Aie/E(B-V) Ratio of extinction at lambda compared to (B-V) color excess --- Synthetic spectra for Case classification Intrinsic spectra for Case classification Synthetic spectra for MK classification Intrinsic spectra for MK classification lambda Wavelength nm F0 Flux for M0 type W/m2/nm F0c Flux in continuum for M0 type W/m2/nm F1 Flux for M1 type W/m2/nm F1c Flux in continuum for M1 type W/m2/nm F2 Flux for M2 type W/m2/nm F2c Flux in continuum for M2 type W/m2/nm F3 Flux for M3 type W/m2/nm F3c Flux in continuum for M3 type W/m2/nm F4 Flux for M4 type W/m2/nm F4c Flux in continuum for M4 type W/m2/nm F5 Flux for M5 type W/m2/nm F5c Flux in continuum for M5 type W/m2/nm F6 Flux for M6 type W/m2/nm F6c Flux in continuum for M6 type W/m2/nm F7 Flux for M7 type W/m2/nm F7c Flux in continuum for M7 type W/m2/nm F8 Flux for M8 type W/m2/nm F8c Flux in continuum for M8 type W/m2/nm F9 Flux for M9 type W/m2/nm F9c Flux in continuum for M9 type W/m2/nm F10 Flux for M10 type W/m2/nm F10c Flux in continuum for M10 type W/m2/nm UNKNOWN 1997 DEC 16 J_A+AS_105_311.xml Radio observations of the Coma cluster of galaxies and its intermediate vicinity. I. Radio data and optical identifications J/A+AS/105/385 J/A+AS/105/385 I. Radio data and optical identifications Radio observations of the Coma cluster of galaxies and its intermediate vicinity. I. Radio data and optical identifications K -T Kim P P Kronberg P E Dewdney T L Landecker Astron. Astrophys. Suppl. Ser. 105 385 1994 1994A&AS..105..385K galaxies: clusters: general galaxies: clusters: individual (Coma cluster) galaxies: magnetic fields intergalactic medium radio continuum: galaxies Continuum radio surveys of a region containing the Coma cluster of galaxies have been made at eight different frequencies with the DRAO and VLA synthesis telescopes. These surveys detected 482 sources above 30 mJy at 408 MHz within a circular region of diameter about 9.7deg and 298 sources in the frequency range 1.3-1.7 GHz within a circular region of diameter 3.1deg. The completeness level of the surveys is 10 mJy at 1.4 GHz for sources located within a 65' radius from the phase centre. 17 new rotation measures were obtained for sources in the field of the Coma cluster. Of 107 sources detected at 1380 MHz with the VLA within 30' radius of its phase centre, 33 sources (31%) are optically identified with galaxies. The number of yet unidentified cluster sources expected from the survey is estimated to be about 20. With the redshift data currently available, only 29 Coma cluster radio galaxies have been identified.
Optical identification RAh Right ascension 1950 (radio position) h RAm Right ascension 1950 (radio position) min RAs Right ascension 1950 (radio position) s e_RA rms uncertainty on RA s DE Declination 1950 (radio position) deg DEm Declination 1950 (radio position) arcmin DEs Declination 1950 (radio position) arcsec e_DE rms uncertainty on DE arcsec 5C 5C denomination --- Name1 Usual name --- F1 Flux density at 1 GHz mJy n_F1 Note on flux density number=1 W = WSRT 610 MHz (Valentijn et al. 1977), + = VLA 1380 MHz, ++ = VLA 1630 MHz, * = DRAO 1420MHz, e = estimated --- e_F1 rms uncertainty on flux density mJy SI Spectral index --- n_SI Note on spectral index number=1 W = WSRT 610 MHz (Valentijn et al. 1977), + = VLA 1380 MHz, ++ = VLA 1630 MHz, * = DRAO 1420MHz, e = estimated --- e_SI rms uncertainty on spectral index --- n_e_F1 Note on rms uncertainty of spectral index number=1 W = WSRT 610 MHz (Valentijn et al. 1977), + = VLA 1380 MHz, ++ = VLA 1630 MHz, * = DRAO 1420MHz, e = estimated --- Maj Size (major axis) arcsec Min Size (minor axis) arcsec PA Position angle deg n_id When *, the following values concerns the second optical identification --- DRA Radio-optical position difference in alpha arcsec DDE Radio-optical position difference in delta arcsec IC Identification quality --- Name2 Optical name --- Type Galaxy type --- Mv Photographic magnitude mag n_Mv Note on photographic magnitude number=1 W = WSRT 610 MHz (Valentijn et al. 1977), + = VLA 1380 MHz, ++ = VLA 1630 MHz, * = DRAO 1420MHz, e = estimated --- V Velocity km/s Ref References number=2 * = Jaffe, et al. (1976), KG = Kent & Gunn (1982), GP = Godwin & Peach (1977) TT = Tift & Tarenchi (1977) --- Patricia Bauer CDS 1994 Feb 18 J_A+AS_105_385.xml Evolutionary sequences of stellar models with very high metallicity. V. Z = 0.10 J/A+AS/105/39 J/A+AS/105/39 Evolutionary sequences V. Evolutionary sequences of stellar models with very high metallicity. V. Z = 0.10 F Fagotto A Bressan G Bertelli C Chiosi Astron. Astrophys. Suppl. Ser. 105 39 1994 1994A&AS..105...39F J/A+AS/100/647 : (II: Z = 0.02) J/A+AS/104/365 : (III: Z = 0.0004 and Z = 0.05) J/A+AS/105/29 : (IV: Z = 0.004 and Z = 0.008) J/A+AS/105/39 : (V: Z = 0.10) Abundances Models, evolutionary stars: evolution stars: interiors We present detailed tabulations of a large grid of stellar models with initial chemical compositions [Y=0.475, Z=0.1] computed with the radiative opacities by Huebner et al. (1977) and convective overshoot. This choice of the opacity is due to the high metallicity in use, because the Livermore Library of radiative opacities (Iglesias et al. 1992) did not contain tabulations for Z=0.1. The tracks span the range of initial masses from 0.6M_{sun}_ to 9M_{sun}_ and extend from the zero age main sequence (ZAMS) till very advanced evolutionary phases. Specifically, low- and intermediate-mass stars are followed either till the white dwarf (WD) or late stages of the early asymptotic giant branch (AGB) phase, depending on the mass of the star and on details of the evolutionary behaviour discussed in the text. Massive stars are calculated till core C-ignition. The critical masses separating low- from intermediate-, and intermediate-mass from massive stars are M_HeF_=1.3M_{sun}_ andM_up_=4M_{sun}_, respectively. All the models are calculated at constant mass. The results for all the models are given in extensive tables which summarize also the lifetimes of the various phases and the variations of the surface abundances limited to the first dredge-up. The stellar models presented here are particularly suited to interpret the CMDs of very metal-rich clusters and the stellar content of elliptical galaxies. However we warn the reader that, because of the opacity, these models are not fully homogeneous with the others of the same series by Bressan et al. (1993) and Fagotto et al. (1994a,b) that are calculated with the Livermore opacity.
Evolutionary sequences of low mass stars up to the tip of the RGB, 0.6<M<1.3, Z=0.10, Y=0.475, Overshoot Evolutionary sequences of low mass stars during the core helium-burning and EAGB phases 0.45<M<1.3, Z=0.10, Y=0.475 Evolutionary sequences of intermediate stars up to the TPAGB or carbon-ignition 1.4<M<9.0, Z=0.10, Y=0.475, Overshoot m Initial mass solMass Age Age of models yr log(L) Total luminosity [solLum] log(Teff) Effective temperature [K] log(G) Surface gravity [cm/s2] log(Tc) Central temperature [K] log(rho_c) Central density [g/cm3] COMP Central abundance (by mass) of hydrogen or helium --- X_C Central abundance of 12C --- X_O Central abundance of 16O --- Conv Fractionary mass of the convective core (inclusive of overshoot) --- Q_disc Fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log(L_H) Hydrogen luminosity [solLum] Q1_H Fractionary mass of the inner border of the hydrogen rich region --- Q2_H Fractionary mass of the outer border of the H-burning region. The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- log(L_He) Helium luminosity [solLum] Q1_He Fractionary mass of the inner border of the He-burning region (when greater than zero He-burning is in a shell). The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- Q2_He Fractionary mass of the upper border of the He-burning region. The boundary is taken as above. --- log(L_C) Carbon luminosity [solLum] log(L_nu) Neutrinos luminosity (absolute value) [solLum] Q_Tmax Fractionary mass of the point where the temperature attains the maximum value --- table1.tex LaTex version of table1 table2.tex LaTex version of table2 table3.tex LaTex version of table3 Patricia Bauer CDS 1994 Jan 20 UNKNOWN UNKNOWN * 22-Oct-1997: table2 completed with missing models of masses from 0.7 to 1.3 J_A+AS_105_39.xml Optical positions of the radio stars observed with the Repsold Meridian Circle at Cerro Calan, National Observatory J/A+AS/105/429 J/A+AS/105/429 Optical positions of the radio stars observed Optical positions of the radio stars observed with the Repsold Meridian Circle at Cerro Calan, National Observatory G Carrasco P Loyola Astron. Astrophys. Suppl. Ser. 105 429 1994 1994A&AS..105..429C astrometry radio continuum: stars reference systems The positions in right ascension and declination of 50 radio stars observed with the Repsold Meridian Circle at Cerro Calan, National Observatory, are presented. The positions of these radio stars are given in the FK5 System, for the epoch of the observation and the equinox J2000.0. The mean internal error of a star position is +/-0.010s and +/-0.10", in right ascension and declination, respectively. The residuals in right ascension and declination of 24 FK5 radio stars and a comparison of the results of 31 radio stars observed at San Fernando and 22 stars observed at La Palma, Spain, are presented.
Radio stars positions for the epoch of observation and equinox J2000.0 N Internal number --- HD HD designation --- V Visual magnitude mag Sp Spectral type --- RAh Right ascension J2000.0 h RAm Right ascension J2000.0 min RAs Right ascension J2000.0 s EPA Epoch-1900 of right ascension (x 100) yr NRA Number of accepted observations in right ascension --- e_RA rms uncertainty on right ascension 0.001s DE- Declination sign --- DEd Declination J2000.0 deg DEm Declination J2000.0 arcmin DEs Declination J2000.0 arcsec EPD Epoch-1900 of declination (x 100) yr NDE Number of accepted observations in declination --- e_DE rms uncertainty on declination 0.01arcsec Name Name of the star --- Differences in alpha and delta "Cerro Calan-FK5" N Identification number --- FK5 FK5 designation --- RA Right ascension h DE Declination deg DeltaRA Cerro Calan-FK5 difference in alpha 0.01arcsec DeltaDE Cerro Calan-FK5 difference in delta 0.01arcsec Differences in alpha and delta "Cerro Calan-San Fernando" and "Cerro Calan-Carlsberg" N Identification number --- Name Usual name --- RA Right ascension h DE Declination deg DRAsf Cerro Calan-San Fernando difference in alpha 0.01arcsec DRAca Cerro Calan-Carlsberg difference in alpha 0.01arcsec DDEsf Cerro Calan-San Fernando difference in delta 0.01arcsec DDEca Cerro Calan-Carlsberg difference in delta 0.01arcsec Patricia Bauer CDS 1994 Feb 18 J_A+AS_105_429.xml Kinematics of 14 early-type galaxies J/A+AS/105/433 J/A+AS/105/433 Kinematics of 14 early-type galaxies Kinematics of 14 early-type galaxies G Longo S Zaggia G Busarello G Richter Astron. Astrophys. Suppl. Ser. 105 433 1994 1994A&AS..105..433L galaxies: elliptical and lenticular, cD galaxies: kinematics and dynamics galaxies: structure We present rotation curves and velocity dispersion profiles at several position angles for 9 ellipticals and 5 early type disk systems. A kinematically decoupled inner component is detected in NGC 1374. Central velocity dispersions are provided for other 3 early-type galaxies.
Kinematical data NGC Name --- PA Position angle deg r radius arcsec v rotation velocity km/s e_v rms uncertainty on rotation velocity km/s Sigma velocity dispersion km/s e_Sigma rms uncertainty on velocity dispersion km/s tables.tex LaTeX version of tables Patricia Bauer CDS 1994 Jun 27 J_A+AS_105_433.xml The V505 Sagittarii system: new B,V photoelectric observations and light curve analysis J/A+AS/105/47 J/A+AS/105/47 The V505 Sagittarii system: new B,V The V505 Sagittarii system: new B,V photoelectric observations and light curve analysis H Rovithis-Livaniou P Rovithis Astron. Astrophys. Suppl. Ser. 105 47 1994 1994A&AS..105...47R binaries: eclipsing stars: individual (V505 Sgr) Photoelectric observations, in B and V, of the system V 505 Sagittarii obtained during 1990, 1991 and 1992 at the Kryonerion Astronomical Station of the National Observatory of Athens, are given. The corresponding light curves (typical Algol-type) were analysed using Budding and Zeilik's program. New photoelectric and absolute elements for the system are given.
B observations HJD Heliocentric Julian Day d Phase Phase --- Delta(mB) Difference in B magnitude mag V observations HJD Heliocentric Julian Day d Phase Phase --- Delta(mV) Difference in V magnitude mag Patricia Bauer CDS 1994 Jan 27 J_A+AS_105_47.xml Binary star speckle measurements during 1989-1993 from the SAO 6 m and 1 m telescopes in Zelenchuk J/A+AS/105/503 J/A+AS/105/503 Binary star speckle measurements during 1989-1993 Binary star speckle measurements during 1989-1993 from the SAO 6 m and 1 m telescopes in Zelenchuk I I Balega Y Y Balega I N Belkin A F Maximov V G Orlov E A Pluzhnik Z U Shkhagosheva V A Vasyuk Astron. Astrophys. Suppl. Ser. 105 503 1994 1994A&AS..105..503B astrometry binaries: visual techniques: interferometric We have continued to survey visual and interferometric binary stars with significant orbital motion by means of speckle method at the telescopes of the Special Astrophysical Observatory (SAO) in Zelenchuk. Here we present the lists of 267 speckle observations made with the 6 m and the 1 m telescopes in the period May 1989-November 1993.
Binary star speckle measurements at the 6 m telescope Binary star speckle measurements at the 1 m telescope ID_numb Star catalogue number --- ID_name Star name --- RAh Right ascension 2000.0 h RAm Right ascension 2000.0 min DE- Declination sign --- DEd Declination 2000.0 deg DEm Declination 2000.0 arcmin Data Epoch of observation d PA Position angle deg u_PA uncertainty flag on position angle --- n_PA A '*' means that the star was not resolved during these observations --- Rho Angular separation arcsec u_Rho uncertainty flag on angular separation --- Patricia Bauer CDS 1994 Jun 21 J_A+AS_105_503.xml Optical Spectra and redshifts of 1 Jy, S4 and S5 radio source identifications.V. J/A+AS/105/67 J/A+AS/105/67 Optical spectroscopy of 1Jy, S4 and S5 sources Optical Spectra and redshifts of 1 Jy, S4 and S5 radio source identifications.V. M Stickel H Kuehr Astron. Astrophys. Suppl. Ser. 105 67 1994 1994A&AS..105...67S III/175 : (gathers papers I-V) J/A+AS/80/103 : (I) J/A+AS/97/483 : (II) J/A+AS/98/393 : (II-Observational data) J/A+AS/100/395 : (III) J/A+AS/101/521 : (IV) J/A+AS/103/349 : (Update of optical identifications) J/A+AS/105/211 : (Optical identification of 1Jy) J/A+AS/115/11 : (Optical identifications from 1Jy, S4, S5) Cross identifications Observatory log Radio sources Redshifts Spectroscopy BL Lacertae objects: general catalogs galaxies: general quasars: general radio continuum: galaxiesl The results of optical spectroscopy are presented for the optical counterparts of 14 radio sources from the 1 Jy, S4, and S5 radio source catalogues. New redshifts are given for eight sources, three uncertain redshifts have been clarified and the redshifts of two sources were confirmed. The remaining source was confirmed as a BL Lac object showing only a featureless spectrum. Additional direct imaging data are provided for three sources.
Observed radio source identifications Object Object name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec m Magnitude of the optical identification mag Type Type of the optical identification --- S_5GHz 5GHz flux Jy s(11-6) two-point spectral index between 11 and 6 cm --- fc References to published Finding Charts number=1 References : 0) this paper 1) Kuehr H. 1977, A&AS 29,139 2) Cohen A.M., Porcas R.W., Browne I.W.A., Daintree E.J., Walsh D. 1977, MemRAS 84, 1 3) Kuehr H., Johnston K.J., Odenwald S., Adlhoch J. 1987, A&AS 71, 493 4) Bolton J.G., Shimmins A.J., Merkelijn J. 1968, Austral. J. Phys. 21, 81 5) Hazard C. 1972, Astrophys. Lett. 11, 139 6) Johnson K.H. 1974, AJ 79, 1006 7) Riley J.M. 1989, MNRAS 238, 1055 8) Fugmann W., Meisenheimer K., Roeser H.-J. 1988, A&AS 75, 173 9) Rieke G.H., Lebofsky M.J., Kinman T.D. 1979, ApJ 213, L151 10) Stickel M., Kuehr H., Fried J.W. 1993a, A&AS 97, 483 11) Kapahi V.K. 1981, A&AS 43, 381 --- Cats Catalogue membership --- Names Other names --- Journal of the observations Object Object name --- Date Observation date --- Tel Telescope number=2 #3.5m = 3.5 m telescope on Calar Alto, Spain #2.2m = 2.2 m telescope on Calar Alto, Spain --- iTime Total Integration time s Scale Scale of the wavelength calibrated spectra 0.1nm/pix Scale2 Scale in in red channel for Twin Spectrograph 0.1nm/pix Identified emission and absorption line features Object Object name --- z Redshift computed from unweighted z_ind --- Id Element identification --- lam_0 Rest wavelength 0.1nm lam_obs Observed wavelength 0.1nm z_ind Individual redshift --- Patricia Bauer CDS 1994 Jan 05 J_A+AS_105_67.xml Atomic data and spectral line intensities for O VIII and Fe XVII resonance lines as well as their O VII and Fe XVI satellite lines J/A+AS/105/77 J/A+AS/105/77 Atomic data and spectral line intensities for O V Atomic data and spectral line intensities for O VIII and Fe XVII resonance lines as well as their O VII and Fe XVI satellite lines M Cornille J Dubau P Faucher F Bely-Dubau C Blancard Astron. Astrophys. Suppl. Ser. 105 77 1994 1994A&AS..105...77C atomic data line: identification Sun: corona Sun: X-rays, gamma rays X-rays: general The atomic data required to analyse low density coronal plasmas have been calculated and used to interpret X-ray spectra observed by the Flat Crystal Spectrometer of the SMM/NASA satellite in the 14-19 A wavelength range. The emission lines correspond mainly to Fe XVI, Fe XVII, Fe XVIII and some ones to O VII, O VIII.
Fe XVII energy levels and radiative transition probabilities Fe XVII energy levels O VIII energy levels and radiative transition probabilities Id. identification number corresponding to the following level --- Level level --- E energy level cm-1 Id.f1 final level of Ar1 --- Ar1 radiative transition probability (first of the two more important) s-1 Id.f2 Final level of Ar2 --- Ar2 radiative transition probability (second of the two more important) s-1 SAr Sum of all radiative probabilities from the level identified in the first two columns s-1 Fe XVII wavelengths and radiative transition probabilities Tran. transition (with identification numbers of table1) --- LambdaObs observed wavelength from Phillips et al. (1982) 0.1nm Lambda1 observed wavelength from this work 0.1nm Lambda2 observed wavelength from Loulergue & Nussbaumer (1975) 0.1nm Ar1 radiative transition probability form this work s-1 Ar2 radiative transition probability form Loulergue & Nussbaumer (1975) s-1 Fe XVII fine structure collision strengths Id. level identification number (form table1) --- Omega70 fine structure collision strength for an electron impact energy of 70 Ry --- Omega85 fine structure collision strength for an electron impact energy of 85 Ry --- Omega200 fine structure collision strength for an electron impact energy of 200 Ry --- Omega400 fine structure collision strength for an electron impact energy of 400 Ry --- Omega600 fine structure collision strength for an electron impact energy of 600 Ry --- Omega800 fine structure collision strength for an electron impact energy of 800 Ry --- Fe XVI dielectronic satellite atomic data O VII dielectronic satellite atomic data Ts autoionizing level s of the transition (s -> f) --- Tf final level f of the transition (s -> f) --- Es energy of the corresponding captured electron Ry lambda wavelength 0.1nm F*2(sf) Fe XVI dielectronic satellite atomic data s-1 n_F*2(sf) relative importance of each F*2(sf) to this one of the strongest dielectronic line choosen as a reference line --- Fe XVI fine structure collision strengths Level excited level --- Omega60 fine structure collision strength for an electron impact energy of 60 Ry --- O VIII fine structure collision strengths Level excited level --- Id. level identification number (see table7) --- Omaga62 fine structure collision strength for an electron impact energy of 62 Ry --- Omaga93 fine structure collision strength for an electron impact energy of 93 Ry --- Omaga124 fine structure collision strength for an electron impact energy of 124 Ry --- Fe XVII line energy differential emissivity and relative differential emissivity </tableLink> </tableLinks> <fields> <field> <name>Tran.</name> <definition>Transition</definition> <units>---</units> </field> <field> <name>Ident.</name> <definition>Identification</definition> <units>---</units> </field> <field> <name>lambda</name> <definition>wavelength</definition> <units>0.1nm</units> </field> <field> <name>Epsilon70</name> <definition>line energy differential emissivity for an electron impact energy of 70 Ry</definition> <units>ph/s/cm3</units> </field> <field> <name>Epsilon85</name> <definition>line energy differential emissivity for an electron impact energy of 85 Ry</definition> <units>ph/s/cm3</units> </field> <field> <name>Epsilon200</name> <definition>line energy differential emissivity for an electron impact energy of 200 Ry</definition> <units>ph/s/cm3</units> </field> <field> <name>Epsilon400</name> <definition>line energy differential emissivity for an electron impact energy of 400 Ry</definition> <units>ph/s/cm3</units> </field> <field> <name>Epsilon600</name> <definition>line energy differential emissivity for an electron impact energy of 600 Ry</definition> <units>ph/s/cm3</units> </field> <field> <name>Epsilon800</name> <definition>line energy differential emissivity for an electron impact energy of 800 Ry</definition> <units>ph/s/cm3</units> </field> <field> <name>DE70/E</name> <definition>relative energy differential emissivity for an electron impact energy of 70 Ry</definition> <units>---</units> </field> <field> <name>DE85/E</name> <definition>relative energy differential emissivity for an electron impact energy of 85 Ry</definition> <units>---</units> </field> <field> <name>DE200/E</name> <definition>relative energy differential emissivity for an electron impact energy of 200 Ry</definition> <units>---</units> </field> <field> <name>DE400/E</name> <definition>relative energy differential emissivity for an electron impact energy of 400 Ry</definition> <units>---</units> </field> <field> <name>DE600/E</name> <definition>relative energy differential emissivity for an electron impact energy of 600 Ry</definition> <units>---</units> </field> <field> <name>DE800/E</name> <definition>relative energy differential emissivity for an electron impact energy of 800 Ry</definition> <units>---</units> </field> </fields> </tableHead> <tableHead> <tableLinks> <tableLink xlink:href="table10b"> <title>O VIII line energy differential emissivity and relative differential emissivity Trans. Transition --- Lambda wavelength 0.1nm Epsilon62 line energy differential emissivity for an electron impact energy of 62 Ry ph/s/cm3 Epsilon93 line energy differential emissivity for an electron impact energy of 93 Ry ph/s/cm3 Epsilon124 line energy differential emissivity for an electron impact energy of 124 Ry ph/s/cm3 DE62/E relative energy differential emissivity for an electron impact energy of 62 Ry --- DE93/E relative energy differential emissivity for an electron impact energy of 93 Ry --- DE124/E relative energy differential emissivity for an electron impact energy of 124 Ry --- Most important Fe XVI inner-shell line energy differential emissivities and relative differential emissivity Trans. transition --- Lambda wavelength 0.1nm Epsilon60 most important inner-shell line energy differential emissivity for an electron impact energy of 60 Ry ph/s/cm3 DE60/E most important relative energy differential emissivity for an electron impact energy of 60 Ry --- CDS 1994 May 19 J_A+AS_105_77.xml A 3.9 GHz survey for declination -1 deg to 0 deg. J/A+AS/106/119 J/A+AS/106/119 3.9GHz survey declination -1 to 0deg A 3.9 GHz survey for declination -1 deg to 0 deg. M G Larionov Yu N Parijskij V I Zhuravlev V N Sidorenkov A B Berlin N A Nizhel'skii Astron. Astrophys. Suppl. Ser. 106 119 1994 1994A&AS..106..119L methods: analytical methods: observational radio continuum: general surveys The first results of the deep search survey over a portion of the celestial sphere with the radio telescope RATAN-600 at several cm-wavelengths are analyzed. The tasks of the survey, its parameters for obtaining a catalogue of 691 radio sources at 3.9 GHz are considered. Also discussed are the methodologies of observations and of data processing.
list of the sources Name Source name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin F3.9GHz Flux density at 3.9 GHz Jy e_F3.9GHz rms uncertainty of F3.9GHz (5*rms) mJy Other Other name --- Patricia Bauer CDS 1994 Mar 23 J_A+AS_106_119.xml Variability of luminous blue variables. I. Intermediate-band photometry J/A+AS/106/141 J/A+AS/106/141 Variability of luminous blue variables. I. Intermed Variability of luminous blue variables. I. Intermediate-band photometry H W W Spoon A De Koter C Sterken H J G L M Lamers O Stahl Astron. Astrophys. Suppl. Ser. 106 141 1994 1994A&AS..106..141S stars: activity stars: early-type stars: emission-line, Be stars: variables: general supergiants An extensive photometric dataset has been compiled for six Luminous Blue Variables (LBVs). The dataset comprises published and unpublished measurements in the Stroemgren, Geneva and Walraven photometric systems. The measurements within each individual system are presented in a uniform manner. Combining observations from these three photometric systems, a V_J_ light curve has been constructed for each LBV. Examination of the light curves reveals variations on widely different magnitude and time scales.
ESO Stromgren photometry Name Star name --- JD Heliocentric Julian day d V Johnson V mag LTPV Stromgren photometry SAAO Stromgren photometry Name Star name --- HJD Heliocentric Julian Date d V Johnson V mag b-y Stromgren b-y mag v-b Stromgren v-b mag u-v Stromgren u-v mag Nc Number of comparison stars used in correction --- Sys LTPV instrumental system ident --- Geneva/Johnson photometry Name star name --- HJD Heliocentric Julian Date d Vg Geneva V mag (U-B)g Geneva U-B mag (V-B)g Geneva V-B mag (B1-B)g Geneva B1-B mag (B2-B)g Geneva B2-B mag (V1-B)g Geneva V1-B mag (G-B)g Geneva G-B mag (B-V)j Johnson B-V derived from Geneva photometry mag VBLUW/Johnson photometry Name Star name --- HJD Heliocentric Julian Date d (V)w Walraven V, log(intensity) mag (V-B)w Walraven V-B, log(intensity) mag (B-U)w Walraven B-U, log(intensity) mag (U-W)w Walraven U-W, log(intensity) mag (B-L)w Walraven B-L, log(intensity) mag E Errorcode --- V Johnson V derived from Walraven photometry mag (B-V)j Johnson B-V derived from Walraven photometry mag Patricia Bauer CDS 1994 Mar 22 J_A+AS_106_141.xml The metal-rich globular cluster NGC 6356 J/A+AS/106/161 J/A+AS/106/161 The metal-rich globular cluster NGC 6356 The metal-rich globular cluster NGC 6356 E Bica S Ortolani B Barbuy Astron. Astrophys. Suppl. Ser. 106 161 1994 1994A&AS..106..161B Galaxy: center globular clusters: individual (NGC 6528) Hertzsprung-Russell (HR diagram) CCD photometry in the VRI and Gunn z bands was obtained for the populous bulge globular cluster NGC 6356. The analysis of the red giant branch indicates that it is metal-rich, intermediate between 47 Tuc and NGC 6528; we estimate [Fe/H]=~-0.4. The red giant clump is clearly detected. The horizontal branch morphology is red and compact. We derive a reddening of E(B-V)=0.24+/-0.04 and a distance d=15.0+/-0.4kpc from the Sun. We also present VI colour magnitude diagrams of 47 Tuc for comparison. NGC 6356 and 47 Tuc are important reference objects for studies of more reddened metal-rich bulge clusters.
NGC 6356 V, I photometry 47 Tuc V, I photometry N Sequence number --- X x pixel coordinate as in Fig. 1 pix Y y pixel coordinate as in Fig. 1 pix V V magnitude mag V-I V-I color mag Patricia Bauer CDS 1994 Feb 11 J_A+AS_106_161.xml Near-IR imaging photometry of NGC 1333: I. the embedded PMS stellar population J/A+AS/106/165 J/A+AS/106/165 Near-IR imaging photometry of NGC 1333: I. the Near-IR imaging photometry of NGC 1333: I. the embedded PMS stellar population C Aspin G Sandell A P G Russell Astron. Astrophys. Suppl. Ser. 106 165 1994 1994A&AS..106..165A circumstellar matter infrared: ISM: continuum infrared: stars ISM: individual (NGC 1333) stars: formation stars: pre-main sequence We present near-IR (NIR) J, H and K mosaic images of the active star forming region associated with the optical reflection nebula NGC 1333. These observations cover an area of 10'x10' and are centered on the energetic outflow source SSV 13. From these data, we have obtained NIR photometry of 134 objects down to a 5{sigma} limiting K magnitude of m_K_=16.2 and a conservative survey completeness limit of m_K_=16.0. With the addition of new optical R and I band CCD photometry, and both (sub)mm line and continuum maps, we analyse and discuss the region's morphology and spatial source distribution with additional reference to existing multi-wavelength data. Within the survey field, NGC 1333-S, we find a significant population of young, PMS stars. Specifically, we consider 55 sources or ~41% of the total stellar population are likely in a PMS evolutionary state. These sources exhibiting clustering in the vicinity of SSV 13 although SSV 13 is not at the cluster centre. The implied stellar PMS population has a range of M_K_ of 0-9 magnitudes and J-K colours of ~1-5. We interpret the data as evidence that i) the embedded population is dominated by relatively low-mass stars i.e. <0.3 M_{sun}_ (~55%), and ii) there exists smaller populations of objects consistent with standard young star classes namely, classical T Tauri stars (~25%), Herbig Ae/Be stars (<10%) and Class I sources (<10%). We demonstrate that an apparent turn-over in the m_K_ luminosity function for all sources in the survey field can be modelled by the combined effect of the survey detection limit and spatially variable extinction over the survey region. This suggests that a combination of a de-reddened sample of PMS star, and a detection limit several magnitudes below the expected faintest m_K_ for those sources is required before inferences can be drawn on the luminosity/mass function. We additionally present the discovery of several new compact nebulous features in the region. Two such objects are possibly associated with SSV 13 and HH 7-11. Almost all of these features are associated with blue-shifted CO in the outflows from IRAS sources in the region. We consider in some detail the usage of NIR photometry and colours in a region of significant extinction, e.g. within the boundaries of molecular clouds, to both determine the evolutionary state of an observed sample of stars and subsequently to characterize them into mass, luminosity, activity and age classes. We discuss and apply several methods to separate a population of embedded young pre-main sequence (PMS) stars from the generally larger population of reddened background galactic sources.
Coordinates of sources in NGC1333-S ASR ASR identification --- Delta_RA Distance from center (ASR 1) arcsec Delta_DE Distance from center (ASR 1) arcsec RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Cross References of sources in NGC1333-S ASR ASR identification --- Note s = stellar, a = associated nebulosity, n = nebulous, d = double --- Name Other name number=1 SSV refers to Strom, Vrba & Strom, 1976, AJ 81, 314, referenced in other papers by SVS --- S86a Reference to table3 of Strom et al. (1986) --- S86b Reference to table4 of Strom et al. (1986) --- S86c Reference to table5 of Strom et al. (1986) --- HJ83 Reference to Herbig and Jones (1983) --- Photometry of sources in NGC1333-S ASR ASR identification --- R R magnitude mag I I magnitude mag J J magnitude mag K K magnitude mag R-I R-I color mag J-H J-H color mag H-K H-K color mag J-K J-K color mag Comparison of SSV-ASR Photometry SSV SSV identification --- ASR ASR identification --- Js SSV J magnitude mag Hs SSV H magnitude mag Ks SSV K magnitude mag (J-H)s SSV J-H color mag (H-K)s SSV H-K color mag Ja ASR J magnitude mag Ha ASR H magnitude mag Ka ASR K magnitude mag (J-H)a ASR J-H color mag (H-K)a ASR H-K color mag Note See Note number=1 1) HH17, diffuse component, possibly close double, companion 20" NNW 2) IRAS5, double, bright diffuse component 3) LkHalpha352a, diffuse component, double 4) Isolated star, associated diffuse component 5) HH6 complex, bright diffuse component 6) SSV13, known to be variable 7) Close companion, diffuse component 8) Close companions 9) Close companions 10) Isolated star 11) Close double 12) LkHalpha 271 13) LkHalpha 351, diffuse component, possible jet --- Implied nature of sources in NGC1333-S ASR ASR identification --- R Consistent reddening (YES, NO, CA, CB) number=1 CA = close-Above the upper reddening vector CB = close-Below the lower reddening vector --- Sp Implied spectral type --- Av Absorption mag (m-M)K Distance modulus mag n_(m-M)K A '-' indicates a range of distance moduli number=2 In the mK-MK column, where a range of values are given e.g. 15.8-10.8, this refers to the range of valid distance moduli when that could be possible given an implied spectral type range (e.g. B8-O5 V) estimated from analysing likely errors on the photometry. Such errors could move the location of the CA and CB stars between the two reddening vectors to a certain maximum extent. This maximum gives the limit of the spectral type range. --- (m-M)K2 Lower limit of distance modulus when n_(m-M)K is not blank mag PMS Possible Pre-Main Sequence? (YES, NO, NEB)(3) --- n_PMS See note number=4 * = implied from m-M > 13.9 == 6kpc a = same as * but using assumed Spectral Type - = m-M < 7.7 + implied AV>5 + = implied from associated Halpha emission o = implied from optical c-c diagram --- Patricia Bauer CDS 1994 Mar 18 J_A+AS_106_165.xml Global mapping B-band photometry of a complete sample of Fornax and Virgo early-type galaxies J/A+AS/106/199 J/A+AS/106/199 'Global mapping' B-band photometry of a complete Global mapping B-band photometry of a complete sample of Fornax and Virgo early-type galaxies N Caon M Capaccioli M D'Onofrio Astron. Astrophys. Suppl. Ser. 106 199 1994 1994A&AS..106..199C galaxies: fundamental parameters galaxies: elliptical and lenticular, cD photometry We present the B-band surface photometry of 19 early-type galaxies of the Virgo cluster, and of 28 galaxies of the same morphological type belonging to the Fornax clusters, obtained through the 'global mapping' technique which couples CCD and photographic plates. Taking into account 33 galaxies already studied by Caon et al. (1990) with the same methodology, the Virgo sample of early-type galaxies is now 80% complete down to B_T_=14. The Fornax sample is 95% complete down to B_T_=15. The geometric and photometric properties of the total sample of 80 galaxies are derived measuring accurate light profiles, ellipticities, position angles and Fourier coefficients of the isophotes. The main sources of errors of the 'global mapping' procedure are reviewed and the effects of seeing discussed. Global galaxian parameters such as total luminosity, effective radius, and effective surface brightness, are computed for the whole sample in a homogeneous way. Our goal is to create an unbiased set of data to be used for investigating the process of galaxy formation and evolution.
B-band photometry Name Object name --- D^1/4 Distance at power 1/4 from center arcsec B(maj) Surface brightness along the major axis (folded) mag/arcsec2 B(min) Surface brightness along the minor axis (folded) mag/arcsec2 Eps Ellipticity --- PA Position angle deg B-band photometry Name Object name --- D^1/4 Distance at power 1/4 from center arcsec B(maj)SW Surface brightness along the major axis (side as coded) mag/arcsec2 B(maj)NE Surface brightness along the major axis (side as coded) mag/arcsec2 B(min)SE Surface brightness along the minor axis (side as coded) mag/arcsec2 B(min)NW Surface brightness along the minor axis (side as coded) mag/arcsec2 Eps Ellipticity --- PA Position angle (measured from N through E) deg Patricia Bauer CDS 1994 Mar 21 J_A+AS_106_199.xml Dumbbell galaxies and multiple nuclei in rich clusters: radio data J/A+AS/106/1 J/A+AS/106/1 Radio data in Dumbbell galaxies Dumbbell galaxies and multiple nuclei in rich clusters: radio data L Gregorini H R De Ruiter P Parma E M Sadler G Vettolani R D Ekers Astron. Astrophys. Suppl. Ser. 106 1 1994 1994A&AS..106....1G galaxies: clusters: general galaxies: elliptical and lenticular, cD radio continuum: galaxies We present radio observations at 6 cm for 93 ACO clusters, in which the brightest member consists of either two galaxies of roughly equal brightness inside a common halo (a dumbbell) or has multiple nuclei. A subsample of 27 dumbbell systems, belonging to a volume-limited sample, was observed with the VLA and ATCA. The remaining clusters were mapped with the VLA. The detection rate in the volume-limited sample is 44%. In all 93 clusters observed 43 brightest cluster members were detected in the radio. Parameters are presented for all the radio sources detected in the cluster fields.
Radio sources in the clusters fields Radio sources identified with the cluster brightest member Name Cluster name number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. --- N Reference number of the source; a letter refers to the different components of the extended sources number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. --- RAh Right ascension 1950.0 number=1 in table4, the right ascension and declination refers to the radio emission peak. See also Note (2) below h RAm Right ascension 1950.0 number=1 in table4, the right ascension and declination refers to the radio emission peak. See also Note (2) below min RAs Right ascension 1950.0 number=1 in table4, the right ascension and declination refers to the radio emission peak. See also Note (2) below s DE- Declination sign number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. --- DEd Declination 1950.0 number=1 in table4, the right ascension and declination refers to the radio emission peak. See also Note (2) below deg DEm Declination 1950.0 number=1 in table4, the right ascension and declination refers to the radio emission peak. See also Note (2) below arcmin DEs Declination 1950.0 number=1 in table4, the right ascension and declination refers to the radio emission peak. See also Note (2) below arcsec l_S6cm limit flag on S6cm number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. --- S6cm Total flux density at 6 cm (5 GHz) not corrected for attenuation effects number=2 in table5, -For non detected radio sources, the right ascension and declination refers to optical position of the dominant galaxy the F value refers to 3 sigma limit for the flux; -For the detected radio sources, the right ascension and declination of the first row refers to optical position of the identified galaxy, in the following rows, the parameters refers to radio parameters -For A3432, the high flux 363.5mJy is likely an error (see "Post-Publication Notes" above) mJy FWHM1 Full Width Half Maximun (FWHM) along major axis of a Gaussian fitting of the source number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. arcsec x An 'x' indicates two values of FWHM along major and minor axes number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. --- l_FWHM2 limit flag for second values of FWHM number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. --- FWHM2 FWHM (along minor axis if x in column 53) number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. arcsec l_PA limit flag on PA number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. --- PA Position angle of a Gaussian fitting the source number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. deg LAS Largest angular size for complex sources number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. arcsec D Distance of the source from the pointing position number= A367: there is a very faint (2 sigma) radio source right at the position of the galaxy. A1791: the radio source is complex, and the galaxy is almost certainly associated with the source. A2854: there is little doubt that the dumbbell system and the radio source are associated, even though the positional coincidence is difficult to judge, due to the absence of a strong, well-defined radio core. A3150: there are three galaxies close to the radio source. This is the only unclear case in the whole sample. The identification should be considered uncertain. A3151: one galaxy falls right inside the double radio source, so the identification is probably correct. A3391: the radio source is complex; a faint core is present and lies close (~5 arcsec) to the eastern galaxy of the dumbbell system, and we therefore consider the radio source associated with this galaxy. A3432: see "Post-Publication Notes" A3532: similar to the case of A1791: one galaxy is in between the two lobes of a double source. The identification is quite likely correct. A3618: the western galaxy is probably the one associated with the radio source. A3706: the radio identification is uncertain due to the very faint radio source associated. arcmin Patricia Bauer CDS 1994 Oct 14 UNKNOWN UNKNOWN *02-Mar-1994: first released *14-Oct-1994: ReadMe modified UNKNOWN UNKNOWN Post-publication Notes: *14-Oct-1994: following a remark by H. Andernach (heinz@adel.univ-lyon1.fr) on the high value (363.5mJy) of the peak flux of A3432, L. Gregorini (GREGORINI@astbo1.bo.cnr.it) answered: "I had no time to directly check on the map (I am teaching), but from my printed paper I agree with you: the correct value must be a factor of 10 less. Thank you for finding this mistake." J_A+AS_106_1.xml Delta Sct stars: a new revised list J/A+AS/106/21 J/A+AS/106/21 Delta Sct stars: a new revised list Delta Sct stars: a new revised list E Rodriguez P Lopez De Coca A Rolland R Garrido V Costa Astron. Astrophys. Suppl. Ser. 106 21 1994 1994A&AS..106...21R delta Scuti stars: oscillations An extensive and up to date list of delta Sct stars is presented. This catalogue is intended to be a comprehensive review of observational characteristics of all the delta Sct stars known until now, including stars contained in earlier catalogues together with other new discovered variables, covering information published until November 1993. Global information in the form of histograms and diagrams are also shown.
Delta Sct stars HD HD designation --- HR Bright stars HR designation --- SAO SAO designation --- BD BD designation --- CD CD designation --- CPD CPD designation --- GCVS GCVS designation --- Other Other designation --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s u_RA When ':' the precision is in arcmin --- DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin Sp Spectral type --- P Period d u_P uncertainty flag on P --- A Amplitude (V) mag V V magnitude or B magnitude (see n_V) mag n_V When B, V contains B magnitude --- B-V B-V colour mag U-B U-B colour mag (b-y) (b-y) colour mag m1 m1 index mag c1 c1 index mag Beta Beta index mag l_vsini limit flag on vsini --- vsini Rotational velocity km/s RV Radial velocity km/s R1 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R2 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R3 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R4 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R5 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R6 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R7 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R8 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R9 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- R10 Reference number=1 The reference list is in the file ref The notes relatives to table1 are in the file note --- N Notes --- Reference list Nb Reference number --- R Reference --- Notes to table1 Nb Note number --- N Note (references below) --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1994 Mar 22 J_A+AS_106_21.xml Stroemgren photometry of F- and G-type stars brighter than V=9.6. I. uvby photometry J/A+AS/106/257 J/A+AS/106/257 Stroemgren photometry of F- and G-type stars bright Stroemgren photometry of F- and G-type stars brighter than V=9.6. I. uvby photometry E H Olsen Astron. Astrophys. Suppl. Ser. 106 257 1994 1994A&AS..106..257O catalogs Galaxy: stellar content solar neighborhood stars: fundamental parameters stars: late-type Within the framework of a large photometric observing program, designed to investigate the Galaxy's structure and evolution, H{beta} photometry is being made for about 9000 stars. As a by-product, supplementary uvby photometry has been made. The results are presented in a catalogue containing 6924 uvby observations of 6190 stars, all south of {delta}=+38deg. The overall internal rms errors of one observation (transformed to the standard system) of a program star in the interval 6.5<V<8.5 are 0.0046, 0.0028, 0.0039, and 0.0056, respectively, in V, b-y, m_1_ , and c_1_ . The catalogue has been compared to two earlier catalogues published within the same observing program.
Catalogue of 110 uvby standards stars HD HD (Henry Draper) designation --- Mult Identification of visual double star components included in the diaphragm --- V transformed to the standard Johnson V mag. mag e_V mean error on V mag b-y b-y mag e_(b-y) mean error on (b-y) mag m1 = (v-b) - (b-y) mag e_(m1) mean error on m1 mag c1 = (u-v) - (v-b) mag e_(c1) mean error on c1 mag w_V weight of V --- w_col weight of 4-colour indices --- NN Number of nights --- D(V) Difference V(standard) - V(transformed) mag D(b-y) Difference (b-y)(st) - (b-y)(tr) mag D(m1) Difference m1(st) - m1(tr) mag D(c1) Difference c1(st) - c1(tr) mag The catalogue HD ? HD (Henry Draper) designation NB! This column may be blank --- Mult Identification of visual double star components included in the diaphragm --- Prog Program star list F = star from A&AS 54, 55 (F-star catalog) G,C,H,Y,O,L or * = star from A&AS 102, 89 number=1 G = G-type star C = Calibration star H = Backup program L = Luyten NGP star Y = Hyades star O = Coma star * = miscellaneous reasons see A&AS 102, 99, sect. 5.1 for details --- DM Durchmusterung identification (BD, CD or CP in bytes 17-18; SZZNNNNN on bytes 19-26; appended letter in byte 27 NB! This column may be blank --- ID Alternative identification --- T Transformation group (see A&AS 102, 94, sects. 4.4 and 5.1) D = GKV group, G or C = GKIII group, % W or blank = BAF group --- V transformed to the standard Johnson V mag. mag e_V mean error on V mag b-y on standard system mag e_(b-y) mean error on (b-y) mag m1 on standard system mag e_(m1) mean error on m1 mag c1 on standard system mag e_(c1) mean error on c1 mag w_V weight of V --- w_col weight of 4-colour indices --- NN Number of nights --- Note * = individual note (see paper) --- Erik Heyn Olsen CDS 1994 Jun 13 Erik H. Olsen <eho@bro835.astro.ku.dk> J_A+AS_106_257.xml Theoretical isochrones from models with new radiative opacities J/A+AS/106/275 J/A+AS/106/275 Theoretical isochrones Theoretical isochrones from models with new radiative opacities G Bertelli A Bressan C Chiosi F Fagotto E Nasi Astron. Astrophys. Suppl. Ser. 106 275 1994 1994A&AS..106..275B Hertzsprung-Russell (HR diagram) stars: evolution stars: fundamental parameters stars: interiors We present large grids of theoretical isochrones for the initial chemical compositions [Z=0.0004, Y=0.23], [Z=0.004, Y=0.24], [Z=0.008, Y=0.25], [Z=0.02, Y=0.28], and [Z= 0.05, Y=0.352] and ages in the range 4 10^6^ yr to 16 10^9^ yr. These isochrones are derived from stellar models computed with the most recent radiative opacities by Iglesias et al. (1992). In addition to this we present another set with chemical composition [Z=0.001, Y=0.23] based on models calculated with the radiative opacities by Huebner et al. (1977). All the stellar models are followed from the zero age main sequence (ZAMS) to the central carbon ignition for massive stars or to the beginning of the thermally pulsing regime of the asymptotic giant branch phase (TP-AGB) for low and intermediate mass stars. For each isochrone, we give the current mass, effective temperatures, bolometric and visual magnitudes, (U-B), (B-V), (V-R), (V-I), (V-J), (V-H), and (V-K) colors, and the luminosity function for the case of the Salpeter law. In addition to this, integrated magnitudes and colors at several characteristic points are also presented together with the mass of the remnant star when appropriate. The main characteristic that makes this set of isochrones very valuable is based on their extension in mass and chemical composition, besides the calculation of late stages of evolution, beyond the red giant tip till the white dwarf stage after the planetary nebula phase.
Model for z=0.0004, Y=0.23 Model for z=0.0010, Y=0.23 Model for z=0.0040, Y=0.24 Model for z=0.0080, Y=0.25 Model for z=0.0200, Y=0.28 Model for z=0.0500, Y=0.352 log(Age) Logarithm of the age yr M Current mass. It is usually increasing along the isochrone, but in the transition from the tip of the RGB to the ZAHB and from the tip of the AGB to the P-AGB phase. The mass is decreased in these transitions according to the effects of mass loss during the RGB phase, and the TP-AGB phase as described in section 3. Sun log(Teff) Logarithm of effective temperature K Mbol Bolometric magnitude mag V Absolute visual magnitude mag (U-B) (U-B) color index mag (B-V) (B-V) color index mag (V-R) (V-R) color index mag (V-I) (V-I) color index mag (V-J) (V-J) color index mag (V-H) (V-H) color index mag (V-K) (V-K) color index mag FLUM Luminosity function for the case of the Salpeter law --- Mwind Real value of the mass after mass loss by stellar wind for massive stars number=1 For massive stars the actual value of the mass is not given by the current mass along the isochrone, but it is derived taking into account mass loss by stellar wind as pointed out in section 2.2 of the text. Of course, for low and intermediate mass stars Mwind is not printed in z*.pst files, and its value is defined as zero in table* files. Only in the youngest isochrones, when massive stars are involved and mass loss by stellar wind is taken into account, the value of Mwind represents the actual mass associated to the corresponding luminosity and effective temperature. Sun z0004.pst Postscript files of table1 ready to print z001.pst Postscript files of table2 ready to print z004.pst Postscript files of table3 ready to print z008.pst Postscript files of table4 ready to print z02.pst Postscript files of table5 ready to print z05.pst Postscript files of table6 ready to print Patricia Bauer CDS 1994 Mar 21 J_A+AS_106_275.xml Three-year monitoring of a sample of flat-spectrum radio sources at 327 MHz. J/A+AS/106/29 J/A+AS/106/29 Three-year monitoring of a sample of flat-spectrum Three-year monitoring of a sample of flat-spectrum radio sources at 327 MHz. T Ghosh G Krishna A P Rao Astron. Astrophys. Suppl. Ser. 106 29 1994 1994A&AS..106...29G active gal. nuclei low frequency variability radio sources: general Results of a 3-year monitoring programme at 327 MHz with the Ooty Synthesis Radio Telescope are presented. The majority of the sample consists of BL Lac objects, high-optical polarization quasars (HPQ) and low-optical polarization quasars (LPQ). In addition, a few known variable sources, GHz-peaked spectrum sources and compact doubles were also added. Including an additional set of 36 control and calibrator sources, a total of 82 sources were observed at roughly 3-month intervals for about 3 years. We find 19 variable and 6 possibly-variable sources. However, the observed variability in the BL Lac-HPQ-LPQ subsamples does not seem to be influenced by their optical properties.
Flux-density measurements for the compact-source sample Flux-density measurements for the control and calibrator sample 3C Standard convention denomination (IAU/3C etc.) --- Clas. Source classification (see text.) --- Name Other name --- l_GAMMA limit flag for GAMMA --- GAMMA Corrected variability index (see text) --- Stat. Statistical significance of the variation (see text) --- com. comment (only in table1) --- Obs1 Epoch of the flux density measurement "DD/MM/YY" F327MHz1 Flux density at 327-MHz mJy e_F327Mhz1 rms uncertainty on F327MHz1 mJy Obs2 Epoch of the flux density measurement "DD/MM/YY" F327MHz2 Flux density at 327-MHz2 mJy e_F327MHz2 rms uncertainty on F327MHz2 mJy Obs3 Epoch of the flux density measurement "DD/MM/YY" F327MHz3 Flux density at 327-MHz3 mJy e_F327MHz3 rms uncertainty on F327MHz3 mJy Obs4 Epoch of the flux density measurement "DD/MM/YY" F327MHz4 Flux density at 327-MHz4 mJy e_F327MHz4 rms uncertainty on F327MHz4 mJy Obs5 Epoch of the flux density measurement "DD/MM/YY" F327MHz5 Flux density at 327-MHz5 mJy e_F327MHz5 rms uncertainty on F327MHz5 mJy Obs6 Epoch of the flux density measurement "DD/MM/YY" F327MHz6 Flux density at 327-MHz6 mJy e_F327MHz6 rms uncertainty on F327MHz6 mJy Obs7 Epoch of the flux density measurement "DD/MM/YY" F327MHz7 Flux density at 327-MHza7 mJy e_F327MHz7 rms uncertainty on F327MHz7 mJy Obs8 Epoch of the flux density measurement "DD/MM/YY" F327MHz8 Flux density at 327-MHza8 mJy e_F327MHz8 rms uncertainty on F327MHz8 mJy Obs9 Epoch of the flux density measurement "DD/MM/YY" F327MHz9 Flux density at 327-MHz9 mJy e_F327MHz9 rms uncertainty on F327MHz9 mJy Patricia Bauer CDS 1994 May 09 J_A+AS_106_29.xml Multifrequency observations of ROSAT selected radio sources J/A+AS/106/303 J/A+AS/106/303 Multifrequency observations of ROSAT sources Multifrequency observations of ROSAT selected radio sources M Neumann W Reich E Fuerst W Brinkmann P Reich J Siebert R Wielebinski J Truemper Astron. Astrophys. Suppl. Ser. 106 303 1994 1994A&AS..106..303N Radio sources X-ray sources galaxies: active radio continuum: galaxies radio continuum: general X-rays: galaxies We report on results of multifrequency radio continuum observations with the Effelsberg 100-m telescope of 234 radio sources which have counterparts in the ROSAT all-sky survey. Observations have been made at 21 cm, 11 cm, 6 cm and 2.8 cm wavelength in the flux density range above 20 mJy. We have determined the spectrum, size, linear polarization and improved positions of these sources. We give the statistical properties of the ROSAT selected radio sources and compare them with results from unbiased radio source surveys so far available.
Data for ROSAT selected radio sources with a position differences of <= 2' Data for ROSAT selected radio sources with a position differences of > 2' RAh Right ascension 2000 of X-ray position h RAm Right ascension 2000 of X-ray position min RAs Right ascension 2000 of X-ray position s DE- Declination sign --- DEd Declination 2000 of X-ray position deg DEm Declination 2000 of X-ray position arcmin DEs Declination 2000 of X-ray position arcsec RA1950h Right ascension 1950 of X-ray position h RA1950m Right ascension 1950 of X-ray position min RA1950s Right ascension 1950 of X-ray position s DE1950- Declination sign --- DE1950d Declination 1950 of X-ray position deg DE1950m Declination 1950 of X-ray position arcmin DE1950s Declination 1950 of X-ray position arcsec DeltaRA (RA_radio - RA_X-ray)*cosDE arcsec DeltaDE DE_radio - DE_X-ray arcsec Counts X-ray counts (0.1 keV =< E =< 2.4 keV) s-1 e_Counts Statistical error of X-ray counts s-1 l_F1476 Limit flag for F1476 --- F1476 Integrated flux density at 1.476 GHz mJy n_F1476 Note for F1476 number=1 A C stands for flux densities which have been taken from the 1.4 GHz catalogue of White, R.L. and Becker, R.H. 1992ApJS...79..331W (also Cat. <VIII/17>) or derived from the 4.85 GHz maps by Condon J.J., Broderick, J.J., Seielstad, G.A. (1989AJ.....97.1064C) --- e_F1476 Error code for F1476 number=2 1(6-9%), 2(9-14%0, 3(14-23%), 4(>23%) --- SE1476a Source extension at 1.476 GHz number=3 0 = point-like, unresolved arcsec --- indicates two values for source extension --- SE1476b Second value of source extension arcsec l_F2695 Limit flag on F2695 --- F2695 Integrated flux density at 2.695 GHz mJy e_F2695 Error code for F2695 number=2 1(6-9%), 2(9-14%0, 3(14-23%), 4(>23%) --- SE2695a Source extension at 2.695 GHz number=3 0 = point-like, unresolved arcsec --- indicates two values for source extension --- SE2695b Second value of source extension arcsec l_DP2695 Limit flag on DP2695 --- DP2695 Degree of polarisation at 2.695 GHz % F4750 Integrated flux density at 4.750 GHz mJy n_F4750 Note for F4750 number=1 A C stands for flux densities which have been taken from the 1.4 GHz catalogue of White, R.L. and Becker, R.H. 1992ApJS...79..331W (also Cat. <VIII/17>) or derived from the 4.85 GHz maps by Condon J.J., Broderick, J.J., Seielstad, G.A. (1989AJ.....97.1064C) --- e_F4750 Error code for F4750 number=2 1(6-9%), 2(9-14%0, 3(14-23%), 4(>23%) --- SE4750a Source extension at 4.750 GHz number=3 0 = point-like, unresolved arcsec --- indicates two values for source extension --- SE4750b Second value of source extension arcsec l_DP4750 Limit flag on DP4750 --- DP4750 Degree of polarisation at 4.750 GHz % l_F1055 Limit flag on F1055 --- F1055 Integrated flux density at 10.55 GHz mJy e_F1055 Error code for F1055 number=2 1(6-9%), 2(9-14%0, 3(14-23%), 4(>23%) --- l_SE1055a Limit flag for SE1055a --- SE1055a Source extension at 10.55 GHz number=3 0 = point-like, unresolved arcsec --- indicates two values for source extension --- SE1055b Second value of source extension arcsec l_DP1055 Limit flag on DP1055 --- DP1055 Degree of polarisation at 10.55 GHz % l_alpha1 Limit flag on alpha1-2 --- alpha1 Radio spectral index alpha_(1476-2695 MHz) number=4 S_nu proportional to nu^alpha^ --- e_alpha1 Rms uncertainty on alpha1 --- alpha2 Radio spectral index alpha_(2695-4750 MHz) number=4 S_nu proportional to nu^alpha^ --- e_alpha2 Rms uncertainty on alpha2 --- l_alpha3 Limit flag on alpha3 --- alpha3 Radio spectral index alpha_(4750-10550MHz)_ number=4 S_nu proportional to nu^alpha^ --- e_alpha3 Rms uncertainty on alpha3 --- FX-ray X-ray energy integrated flux density mW/m2 EpX-ray Epoch of X-ray observation yr noEpoch When 'NEP', no epoch of observation --- l_Fradio Limit flag on Fradio --- Fradio Radio frequency integrated flux density mW/m2 EpRadio1 epoch of simultaneous radio observations at >= 2695 MHz yr --- indicates an interval of observations --- EpRadio2 Second epoch of simultaneous radio yr EF EF designation --- Name Other names number=5 references to other names designation: ABCG Abell, G.O.: 1958ApJS....3..211A (cat. <VII/4>) ASI Barbieri, C., Capaccioli, M., Cristiani, S., Nordon, G., Omizzolo, A.: 1982, Mem.S.A.It. 53, 511 (1982MmSAI..53..511B) B2.1 Colla, G., Fanti, C., Fanti, R., Ficarra,A., Formiggini, L., Gandolfi, E., Grueff, G. et al.: 1970A&AS....1..281C (Cat. <VIII/36>) B2.2 Colla, G., Fanti, C., Fanti, R., Ficarra,A., Formiggini, L., Gandolfi, E., Lari et al.: 1972A&AS....7....1C (Cat. <VIII/36>) B2.3 Colla, G., Fanti, C., Fanti, R., Ficarra,A., Formiggini, L., Gandolfi, E., Gioia, I. et al: 1973A&AS...11..291C (Cat. <VIII/36>) B2.4 Fanti, C., Fanti, R., Ficarra, A., Padrielli, L.: 1974A&AS...18..147F (Cat. <VIII/36>) B3 Ficarra, A., Grueff, G., Tonassetti, G.: 1985A&AS...59..255F (Cat. <VIII/37>) BC Barbieri, C., Capacciolo, M.: 1974, Publ.Oss.Astr.Padova BOZ Bozyan, E.P.: 1979AJ.....84..910B BUR Burbidge, E.M.: 1967ApJ...149L..51B BYS Bystedt, J.E.V.: 1975A&A....39..155B 3C Edge, D.O., Shakeshaft, J.R., McAdam, W.B., Baldwin, J.E. Archer, S.: 1959, Memoirs R.A.S. 68, 37 (1959MmRAS..68...37E) 4C Pilkington, J.D.H., Scott, P.F.: 1965, Memoirs R.A.S. 69, 183 (1965MmRAS..69..183P); Gower, J.F.R., Scott, P.F., Wills, D.: 1967, Memoirs R.A.S. 71, 49 (1967MmRAS..71...49G) 5C Kenderline, S., Ryle, M., Pooley, G.G.: 1966MNRAS.134..189K Pooley, G.G., Kenderline, S.: 1968MNRAS.139..529P Pooley, G.G.: 1969MNRAS.144..101P Willson, M.A.G.: 1970MNRAS.151....1W Pearson, T.J.: 1975MNRAS.171..475P CHJ Condon, J.J., Hicks, P.D., Jauncey, D.L.: 1977AJ.....82..692C CPB Cohen, A.M., Porcas, R.W., Browne, I.W.A., Daintree, E.J., Walsh, D.: 1977, Memoirs R.A.S. 84, 1 (1977MmRAS..84....1C) CTA Harris, D.E., Roberts, J.A.: 1960PASP...72..237H DON Donivon, F.F., Pollock, J.T., Smith, A.G., Leacock, R.J., Scott, R.I., Edwards, P.L., Gearhart, M.R.: 1978PASP...90...24D EKM Edwards, T., Kronberg, P.P., Menard, G.: 1975AJ.....80.1005E GB Maslowski, J.: 1972, Acta Astron. 22, 227 (1972AcA....22..227M) HB1 Hewitt, K., Burbidge, G.: 1991ApJS...75..297H (Cat. <VII/178>) HB2 Hewitt, K., Burbidge, G.: 1993ApJS...87..451H (Cat. <VII/158>) HOLM Holmberg, E.: 1937, Lund Annals 6 (1937AnLun...6....1H) IRAS F Moshiv, M., Kopan, G., Conrow, T., Maccallou, H., Hacking, P., Greorch, D., et al.: 1990, IRAS Faint Source Catalogue (Cat. <II/126>) K. Kuehr, H.: 1980, PHD-Thesis Bonn KAP Kapahl, V.K.: 1979A&A....74L..11K LON Longair, M.S., Gunn, J.E.: 1975MNRAS.170..121L LRWRM Loiseau, N., Reich, W., Wielebinski, R., Reich, P., Muench, W: 1988A&AS...75...67L MCG Vorotsov-Velyaminov, B.A., Arhipova, V.P.: 1962-1974, Morphological catalogue of Galaxies, Moscow, State University (Cat. <VII/62>, <VII/100>) MER Merkelijn, J.K.: 1968, Aust. J. Phys. 21, 903 MG Lawrence, C.R., Bennett, C.L., Garcia-Barreto, J.A., Greenfield, P.E., Burke, B.F.: 1983ApJS...51...67L Bennett, C.L., Lawrence, C.R., Burke, B.F, Hewitt, J.N., Mahoney, J.: 1986ApJS...61....1B Lawrence, C.R., Bennett, C.L., Hewwitt, J.N., Langston, G.I., Klotz, S.E., Burke, B.F., Turner, K.L.: 1986ApJS...61..105L MRK Markarian, B.E.: 1967, AfZ 3, 55 Markarian, B.E.: 1969a, AfZ 5, 443 Markarian, B.E.: 1969b, AfZ 5, 581 Markarian, B.E.: 1971, AfZ 7, 229 Markarian, B.E., Lipovetskii, V.A.: 1972, AfZ 8, 89 Markarian, B.E., Lipovetskii, V.A.: 1973, AfZ 9, 487 Markarian, B.E., Lipovetskii, V.A.: 1974, AfZ 10, 307 (See Cat. <VII/172>) MS Stocke, J.T., Morris, S.L., Gioia, I.M., Maccucoro, T., Schild, R., Wolter, A.et al.: 1991ApJS...76..813S MW Willson, M.A.G.: 1972MNRAS.156....7W NGC Sulentic, J.W., Tift, W.G: 1973, The revised new General Catalogues, The University of Arizona Press (Cat. <VII/1>) NRAO Pauliny-Toth, I.I.K., Wade, C.M., Heeschen, D.S.: 1966ApJS...13...65P OB-OT Scheer, D.J., Kraus, J.D.: 1967AJ.....72..536S Dixon, R.S., Kraus, J.D.: 1968AJ.....73..381D Fitch, L.T., Dixon, R.S., Kraus, J.D.: 1969AJ.....74..612F Ehman, J.R., Dixon, R.S., Kraus, J.D.: 1970AJ.....75..351E Kraus, J.D., Andrew, B.H.: 1971AJ.....76..103K Brundage, R.K., Dixon, R.S., Ehman, J.R., Kraus, J.D.: 1971AJ.....76..777B Ehman, J.R., Dixon, R.S., Ramakrishna, C.M., Kraus, J.D.: 1974AJ.....79..144E Rinsland, C.P., Dixon, R.S., Gearhart, M.R., Kraus, J.D.: 1974AJ.....79.1129R Rinsland, C.P., Dixon, R.S., Kraus, J.D.: 1975AJ.....80..759R OLS Olsen, E.T.: 1970AJ.....75..764O PG Green, R.F., Schmidt, M., Liebert, J.: 1986ApJS...61..305G (Cat. <II/207>) PGC Patuel, G., Fouque, P., Bottinelli, L., Gouguenheim, L.: 1989A&AS...80..299P (Cat. <VII/119>) PHL Haro, G., Luyten, W.J.:1962, Bol.Obs.Ton. y Tacubaya Vol.3, No. 22, 37 (1962BOTT....3...37H) PKS See Cat. <VIII/15> Bolton, J.G., Gardener, F.F., Mackey, M.B.: 1964, Aust.J.Phys. 17, 340 Price, R.M., Milne, D.K.: 1965, Aust. J. Phys. 18, 329 Day, G.A., Shimmins, A.J., Ekers, R.D., Cole, D.J.: 1966, Aust.J.Phys. 19, 35 Shimmins, A.J., Day, G.A., Ekers, R.D., Cole, D.J.: 1966, Aust.J.Phys. 19, 837 Shimmins, A.J., Day, G.A.: 1968, Aust.J.Phys. 21, 377 Ekers, J.A. (edt.): 1969, Aust.J.Phys. Astrophys.Suppl. 7 Wall, J.V., Shimmins, A.J., Merkelijn, J.K.: 1971, Aust.J.Phys. Astrophys.Suppl. 19 Shimmins, A.J.: 1971, Aust.J.Phys. Astrophys.Suppl. 21 Shimmins, A.J., Bolton, J.G.T: 1972, Aust.J.Phys. Astrophys.Suppl. 26 Bolton, J.G., Shimmins, A.J.: 1973, Aust.J.Phys. Astrophys.Suppl. 30 Shimmins, A.J., Bolton, J.G.: 1974, Aust.J.Phys. Astrophys.Suppl. 32 Bolton, J.G., Shimmins, A.J., Wall, J.V.: 1975, Aust.J.Phys. Astrophys.Suppl. 34, 1 Bolton, J.G., Buttler, P.W.: 1975, Aust.J.Phys. Astrophys.Suppl. 34, 33 Wall, J.V., Shimmins, A.J., Bolton, J.G.: 1975, Aust.J.Phys. Astrophys.Suppl. 34, 55 Shimmins, A.J., Bolton, J.G., Wall, J.V.: 1975, Aust.J.Phys. Astrophys.Suppl. 34, 63 Wall, J.V., Boldon, J.G. Wright, A.E., Savage, A., Hagen, J.V.: 1976, Aust.J.Phys. Astrophys.Suppl. 39, 1 Wright, A.E., Savage, A., Bolton, J.G.: 1977, Aust.J.Phys. Astrophys.Suppl. 41, 1 Savage, A., Bolton, J.G., Wright, A.E.: 1977, Aust.J.Phys. Astrophys.Suppl. 44, 1 Bolton, J.G., Savage, A., Wright, A.E.: 1979, Aust.J.Phys. Astrophys.Suppl. 46, 1 PUB Porcas, R.W., Urry, C.M., Browne, I.W.A., Daintree, E.J., Walsh, D.: 1980MNRAS.191..607P SAR Sargent, W.L.W.: 1977ApJ...212L.105S SBW Shimmins, A.L., Bolton, J.G., Wall, J.V.: 1975, Austr.J.Phys. Astrophys. N34, 63 SHB Smith-Haenni, A.L.: 1977A&AS...27..205S SJE Smith, P.S., Jannuzi, B.T., Elston, R.: 1991ApJS...77...67S STK Stickel, M., Kuehr, H.: 1993A&AS..101..521S (Cat. <III/175>) STI Stickel, M.: 1993, priv. communication STICK Stickel, et al.: 1993, AAS submitted UGC Nilson, P.: 1973, Uppsala General catalogue of galaxies, Nova Acta Regiae Soc. Scient. Ser.V, 1, Uppsala (Cat. <VII/26>) WAM Wampler, E.J., Burke, W.L., Gaskell, C.M., Baldwin, J.A.: 1983, ESO reprint N233 WK Windram, M.D., Kenderline, S. 1969MNRAS.146..265W VV Veron-Cetty, M.P., Veron, P.: 1983A&AS...53..219V (Cat. <VII/54>) WW Wills, D., Wills, B.J.: 1976ApJS...31..143W WWD Wills, D., Wills, B.J., Douglas, J.N.: 1985, in preparation WYN Wyndham, J.D.: 1966ApJ...144..459W ZWG Zwicky, F., Herzog, E.: 1961-1968, Catalogue of galaxies and clusters of galaxies, Vol.I-IV (Cat. <VII/190>) Zwicky, F., Karpowicz, M., Koval, C.T.: 1968, Catalogue of galaxies and clusters of galaxies, Vol.V Zwicky, F., Koval, C.T.: 1968, Catalogue of galaxies and clusters of galaxies, Vol.VI 1-7ZW Zwicky, F.: 1961-1968, Seven privately circulated lists --- tables.tex LaTeX version of tables 2 and 3 Patricia Bauer CDS 1994 Apr 15 J_A+AS_106_303.xml Observations of the Sun during 1993 with the astrolabe of Santiago J/A+AS/106/327 J/A+AS/106/327 Observations of the Sun during 1993 with the Observations of the Sun during 1993 with the astrolabe of Santiago F Noeel Astron. Astrophys. Suppl. Ser. 106 327 1994 1994A&AS..106..327N astrometry Sun: general A program of solar observations at 30deg and 60deg zenith distance is in progress since 1990 with the modified Danjon astrolabe of Santiago. Results in right ascension, Y and apparent semi-diameter of the Sun obtained with the modified Danjon astrolabe at Santiago, are given for 1993.
Astrolabe of Santiago: results of Sun observations, 1993. Zenith distance = 30 deg Astrolabe of Santiago: results of Sun observations, 1993. Zenith distance = 60 deg Date Date of observation (year, month, day) --- MJD Modiufied julian day d EUB Zenith distance residual given by the observation of the Sun east upper border arcsec ELB Zenith distance residual given by the observation of the Sun east lower border arcsec WLB Zenith distance residual given by the observation of the Sun west lower border arcsec WUB Zenith distance residual given by the observation of the Sun west upper border arcsec dAlpha Right ascension (observed-ephemeris) s e_dAlpha rms uncertainty on dAlpha s Y dz + d{delta} cos S, where dz = Zenith distance (observed-adopted), d{delta} = Declination (observed-ephemeris), S = sun paralactic angle (Chollet & Noel, 1993) arcsec dD Sun semi-diameter arcsec e_dD rms uncertainty on Y and dD arcsec DR Observed Sun apparent semi-diameter reduced to the geocenter and to the astronomical unit arcsec Patricia Bauer CDS 1994 Jul 28 J_A+AS_106_327.xml Deep photometry in the core of the open cluster NGC 5606 J/A+AS/106/339 J/A+AS/106/339 Photometry of open cluster NGC 5606 Deep photometry in the core of the open cluster NGC 5606 R A Vazquez G Baume A Feinstein P Prado Astron. Astrophys. Suppl. Ser. 106 339 1994 1994A&AS..106..339V Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 5606) stars: luminosity function, mass function The center of the open cluster NGC 5606 has been re-observed with broad band UBVRI CCD photometry. Up to V = 18.5 likely cluster members are found underlining a sharp but not so populated cluster sequence. With this new photometry the cluster distance modulus is stated in V_0_-M_v_=11.90 (d=2400pc). The mean colour excess reaches the value <E_B-V_>=0.51. The age of the cluster from the isochrone fitting is between 6.3x10^6^ and 7x10^6^ y. Surprisingly enough there are not many stars found below V=15.5 in spite of the fact that we are observing the very core of the cluster. This lack of faint cluster stars produces in turn a flat slope for the cluster mass spectrum. In this respect our computation yields x=1.09 far enough of x=1.35 which is assumed to be the slope characterizing the mass spectrum of galactic stars.
Observed colours and magnitudes in NGC 5606 Nb Adopted sequential number --- V&F Vasquez & Feinstein identification number --- X X position pix Y Y position pix V V magnitude mag u_V uncertainty flag on V number=1 A colon (:) suggests combined errors from 0.07 to 0.10, a double colon (::) indicates errors larger than 0.10. --- U-B U-B colour mag u_U-B uncertainty flag on U-B number=1 A colon (:) suggests combined errors from 0.07 to 0.10, a double colon (::) indicates errors larger than 0.10. --- B-V B-V colour mag u_B-V uncertainty flag on B-V number=1 A colon (:) suggests combined errors from 0.07 to 0.10, a double colon (::) indicates errors larger than 0.10. --- V-R V-R colour mag u_V-R uncertainty flag on V-R number=1 A colon (:) suggests combined errors from 0.07 to 0.10, a double colon (::) indicates errors larger than 0.10. --- V-I V-I colour mag u_V-I uncertainty flag on V-I number=1 A colon (:) suggests combined errors from 0.07 to 0.10, a double colon (::) indicates errors larger than 0.10. --- Patricia Bauer CDS 1994 Jul 28 J_A+AS_106_339.xml Simultaneous multirange observations and detection of rapid variability of BL Lacertae objects J/A+AS/106/361 J/A+AS/106/361 Simultaneous multirange observations and detection of Simultaneous multirange observations and detection of rapid variability of BL Lacertae objects G Z Xie K H Li Y H Zhang F K Liu J H Fan J C Wang Astron. Astrophys. Suppl. Ser. 106 361 1994 1994A&AS..106..361X BL Lacertae objects: general infrared: galaxies The optical (BVRI) and infrared monitoring data covering 2 years for 10 radio-selected BL Lac objects and the simutaneous observations of optical and infrared for BL Lac and 3C 66A are presented here. Seven sources exhibit short time-scale variability, and two sources exhibit medium time-scale variability.
Results of CCD photometry of BL Lac objects Name BL Lac object name --- Date UT date "DD/MM/YY" HD Juilan day d mag magnitude mag e_mag rms uncertainty on mag mag Color Color of the magnitude --- Infrared observations Name BL Lac object name --- Date UT date "DD/MM/YY" JD Julian day d K K magnitude mag e_K rms uncertainty on K mag H H magnitude mag e_H rms uncertainty on H mag J J magnitude mag e_J rms uncertainty on J mag Patricia Bauer CDS 1994 Mar 21 J_A+AS_106_361.xml UBV photometry of the contact binary AB Andromedae J/A+AS/106/373 J/A+AS/106/373 AB And UBV photometry UBV photometry of the contact binary AB Andromedae O Demicran E Derman A Akalin S Selam Z Mueyesseroglu Astron. Astrophys. Suppl. Ser. 106 373 1994 1994A&AS..106..373D binaries: close photometry stars: individual (AB And) New UBV observations of a contact binary AB And obtained during 1988, 1989, 1990, 1991 and 1992 observing seasons at the Ankara University Observatory are presented. Sixteen new (nine primary and seven secondary) times of minimum light were obtained. The new times of minima reveal the following improved light elements: Min I = HJD 2448513.54325(+/-0.00020)+0.33189044(+/-0.00000025)E
1989-1992 observations of AB And HJD Heliocentric Julian day d P Phase --- DVo Differential measurement in V magnitude number=1 Differential measurement in the sense variable minus comparison, after the correction for differential atmospheric extinction mag DBo Differential measurement in B magnitude number=1 Differential measurement in the sense variable minus comparison, after the correction for differential atmospheric extinction mag DUo Differential measurement in U magnitude number=1 Differential measurement in the sense variable minus comparison, after the correction for differential atmospheric extinction mag Patricia Bauer CDS 1994 Mar 21 J_A+AS_106_373.xml Measurements of double stars made at Nice observatory. New doubles stars (24th series) discovered at Nice with the 50cm refractor. J/A+AS/106/377 J/A+AS/106/377 Double star measurements Measurements of double stars made at Nice observatory. New doubles stars (24th series) discovered at Nice with the 50cm refractor. P Couteau R Gili Astron. Astrophys. Suppl. Ser. 106 377 1994 1994A&AS..106..377C binaries: general high resolution Table 1 gives 1182 measurements of 682 binaries observed with the 74 and 50 cm refractors. Table 2 lists 26 new binaries discovered with the 50 cm refractor.
Double stars measurements Ident. ADS, BD or AC identification --- Nom Couple name --- mv total visual magnitude mag Jpos J2000 position --- date Observation epoch yr theta position angle deg n_theta A '-' indicates a range of position angle; for other symbols, see number=1 S = Simple (Simple) PS = Pas simple (Not simple) * = Trop diff. Pas simple (very difficult) ** = Parait simple (looks simple) PV = Pas vu (not seen) PB = Pas vu B (B not seen) D1 = Debut 1er Q (beginning 1st quadrant) TS = Tres serre (very close) --- theta2 Second position angle when n_theta = '-' deg rho Separation angle arcsec u_rho rms uncertainty on rho --- n_rho Quadrant indication number=2 #1Q = first quadrant, 2Q = second quadrant #3Q = third quadrant, 4Q = last quadrant --- md magnitude difference or magnitude of the faintest star if u_md = '-' --- u_md rms uncertainty on md A '-' indicates that the individual magnitudes are given --- mv2 magnitude of the brightest star --- Nobs Observation nights number followed by N for 74cm instrument and n for 50cm instrument --- n_Nobs '(60)' indicates that the great instrument have been diaphragmed at 60cm --- Obs Observator initial: C for Couteau, G for Gili --- R Remarks --- New double stars (24th series) Name Couple name --- Pos alpha-delta 1900-2000 position number=1 #01411-474N5043-73 correspond to RA = 01411, DE = 5043 epoch 1900 and RA = 01474, DE = 5073 epoch 2000 --- BD BD or AC identification --- mv total visual magnitude mag u_mv uncertainty flag on mv --- Sp spectral type --- pm1 proper motion of the first star arcsec pm2 proper motion of the second star arcsec Circ. Reference to the IAU circular No 26 --- Date Observation epoch yr theta Position angle deg u_theta uncertainty flag on theta --- rho Separation angle arcsec u_rho uncertainty flag on rho --- mgn1 Magnitude of the faintest star --- mgn2 Magnitude of the brightest star --- Nobs Observation nights number following by n for the 50 cm instrument --- R COU 2684 Hip 41739 V 7.458 (B-V)+0.422, COU 2689 Hip 67989 V 9.00 (B-V)+0.61 --- Patricia Bauer CDS 1994 Mar 21 J_A+AS_106_377.xml Second Astrolabe Catalogue of Santiago J/A+AS/106/441 J/A+AS/106/441 Second catalogue Santiago Second Astrolabe Catalogue of Santiago F Noeel Astron. Astrophys. Suppl. Ser. 106 441 1994 1994A&AS..106..441N astrometry reference systems Positions for 350 FK5 and 164 FK5 Extension stars as determined with the Danjon astrolabe of Santiago and differences astrolabe-catalogue are given for Equinox J2000.0 and for the mean observation epoch of each star. The average mean error in alpha is +/-0.005s and +/-0.07" in delta. The mean epoch of observation of the catalogue is J1979.96.
Second astrolabe catalogue of Santiago No Astrolabe catalogue star number --- FK5 FK5 number --- V Magnitude of the star (FK5) mag Sp Spectral type (FK5) --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DeltaRA Difference Astrolabe-FK5 in right ascension s e_DeltaRA Mean error of DeltaRA s n_DE A "*" indicates no values for declination --- DE- Sign of declination --- DE Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec DeltaDE Difference Astrolabe-FK5 in declination arcsec e_DeltaDE Mean error of DeltaDE arcsec Obs Julian year, mean epoch of observation - 1900 yr Patricia Bauer CDS 1994 Apr 22 J_A+AS_106_441.xml Near-infrared and optical broadband surface photometry of 86 face-on disk dominated galaxies. I. Selection, observations and data reduction. J/A+AS/106/451 J/A+AS/106/451 Face-on disk galaxies photometry. I. Near-infrared and optical broadband surface photometry of 86 face-on disk dominated galaxies. I. Selection, observations and data reduction. R S De Jong P C Van Der Kruit Astron. Astrophys. Suppl. Ser. 106 451 1994 1994A&AS..106..451D Photometry, infrared Photometry, surface galaxies: fundamental parameters galaxies: photometry galaxies: spiral galaxies: structure surveys We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies. Note: Corrections from erratum in A&AS 107, 419, concerning table7, are included
Optical observations calibration coefficients Near-IR observations calibration coefficients Date Observation period --- Color BVRIHKK' colors --- C0 Zero-point coefficient --- e_C0 rms uncertainty on C0 --- C1 color coefficient --- e_C1 rms uncertainty on C1 --- C2 airmass coefficient --- e_C2 rms uncertainty on C2 --- Observed galaxies global UGC/RC3 parameters UGC UGC denomination --- Name Other name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Delcination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg UGCclass UGC classification --- RC3class RC3 classification --- Dmaj red UGC major axis diameter arcmin b/a red UGC minor over major axis diameter ratio --- VGSR receding velocity km/s Observation log of optical observations Observation log of near-IR observations UGC UGC denomination --- Band BVRIHKK' colors --- Obs Observation date "DD/MM/YY" Np Number of position of observation --- ExpTime Exposition time per position s Qual Photometric quality number=1 Photometric quality is defined as: 1: photometric 2: 0.0-0.2 mag 3: 0.2-0.5 mag 4: 0.5-1.0 mag 5: >1.0 mag --- Seeing FWHM seeing arcsec Notes See note number=2 1: Driftscan 2: Internal calibration 3: Calibrated using Longo and de Vaucouleurs (1983) 4: Mosaic 5, 7: JKT, GEC CCD, 0.6arcsec pixels 6, 8: JKT, RCA CCD, 0.41arcsec pixels 9: INT, GEC CCD, 0.54arcsec pixels 10: INT, EEV CCD, 0.53arcsec pixels 11: 1.3m MDM observatory, Thomson CCD, 0.48arcsec pixels --- BVRIHK PA, b/a and integrated magnitudes UGC UGC denomination --- PA Position angle deg b/a major over minor axis ratio --- mB B magnitude mag e_mB rms uncertainty on mB mag mV V magnitude mag e_mV rms uncertainty on mV mag mR R magnitude mag e_mR rms uncertainty on mR mag mI I magnitude mag e_mI rms uncertainty on mI mag mH H magnitude mag e_mH rms uncertainty on mH mag mK K magnitude mag e_mK rms uncertainty on mK mag Surface brightness at UGC radii and radii at 25 B-mag/arcsec2 and 23.5 R-mag/arcsec2 UGC UGC denomination --- Mu.B Surface brightness measured at the blue UGC diameter mag/arcsec2 e_Mu.B rms uncertainty on Mu.B mag/arcsec2 Mu.R Surface brightness measured at the red UGC diameter mag/arcsec2 e_Mu.R rms uncertainty on Mu.R mag/arcsec2 DB25/2 Isophotal major axis radius at 25 B-mag/arcsec2 arcsec e_DB25/2 rms uncertainty on DB25/2 arcsec DR23.5/2 Isophotal major axis radius at 23.5 R-mag/arcsec2 arcsec e_DR23.5/2 rms uncertainty on DR23.5/2 arcsec Observational parameters UGC Galaxy name --- n_UGC "N2" when second extraction number=1 N2 indicates that the luminosity profiles have been extracted again, using only the area common to all frames. As the area observed in the near-IR was in general smaller, these files should be used to generate color profiles. Only UGC438N2 and UGC10445N2 indicate a second set of independent observations. --- Incl Inclination deg PA Position angle deg Band Band where the data where measured --- ExpTime Total exposure time s MagOff Magnitude zero-point offset mag MagSky Surface brightness of the sky mag e_MagSky rms uncertainty on MagSky mag MagTot Apparent magnitude of the galaxy mag e_MagTot rms uncertainty on MagTot mag Seeing FWHM seeing arcsec Date Observatrion date ---- Phot Estimated photometric quality number=2 The photometric quality is 1) photometric 2) 0.0-0.2 mag error 3) 0.2-0.5 mag error 4) 0.5-1.0 mag error 5) >1.0 mag error --- Surface brightness profiles (Fig.12 in the paper) UGC Galaxy name, as in "params" --- n_UGC "N2" when second extraction, as in "params" --- Row Row number --- Rad Radius at which the surface brightness was measured arcsec Mu.B Surface brightness in B band mag/arcsec2 Mu.V Surface brightness in V band mag/arcsec2 Mu.R Surface brightness in R band mag/arcsec2 Mu.I Surface brightness in I band mag/arcsec2 Mu.H Surface brightness in H band mag/arcsec2 Mu.K Surface brightness in K band mag/arcsec2 Patricia Bauer, Francois Ochsenbein CDS 1995 Jul 24 UNKNOWN UNKNOWN * 07-Sep-1994: archived table1 to table7 * 11-Mar-1995: surface profile files kindly provided by R.S. de Jong (R.S.deJong@durham.ac.uk) * 24-Jul-1995: Description File standardized J_A+AS_106_451.xml A catalogue of HeII 4686 line intensities in Galactic planetary nebulae J/A+AS/106/559 J/A+AS/106/559 HeII4686 line intensities of PN A catalogue of HeII 4686 line intensities in Galactic planetary nebulae R Tylenda G Stasinska A Acker B Stenholm Astron. Astrophys. Suppl. Ser. 106 559 1994 1994A&AS..106..559T catalogs planetary nebulae: general stars: AGB and post-AGB stars: fundamental parameters We have compiled the intensities of the HeII 4686 lines measured in Galactic planetary nebulae. We present a few observational diagrams related to this parameter, and discuss them with the help of theoretical diagrams obtained from simple model planetary nebulae surrounding evolving central stars of various masses. We determine the hydrogen and helium Zanstra temperature for all the objects with accurate enough data. We argue that, for Galactic planetary nebulae as a whole, the main cause for the Zanstra discrepancy is leakage of stellar ionizing photons from the nebulae.
Intensities of HeII4686 and Halpha for Galactic planetary nebulae PNG PNG number of the planetary nebulae from the Strasbourg-ESO catalogue --- Name Usual name of the planetary nebulae --- l_HeII Limit flag for HeII 4686 intensity --- HeII Intensity of HeII 4686 on the scale Hbeta=100 --- u_HeII Uncertainty flag on HeII 4686 intensity --- r_HeII Short references for HeII 4686 (full references in the paper) number=1 References to Table 1 are: A78 - Ahern 1978 AC79 - Aller & Czyzak 1979 AC83 - Aller & Czyzak 1983 AK87 - Aller & Keyes 1987 AS - Acker-Stenholm survey ASH84 - Adams et al. 1984 B78 - Barker 1978 B80 - Barker 1980 B86 - Barker 1986 B88 - Barker 1988 BC84 - Barker & Cudworth 1984 CPT87 - Clegg et al. 1987 CSP83 - Clegg et al. 1983 CRB91 - McCarthy et al. 1991 DHT90 - Dopita et al. 1990 FP91 - de Freitas Pacheco et al. 1991 FP92 - de Freitas Pacheco et al. 1992 GMC85 - Gutierrez-Moreno et al. 1985 HM78 - Hawley & Miller 1978 K76 - Kaler 1976a K76b - Kaler 1976b K80 - Kaler 1980 K83a - Kaler 1983a K83b - Kaler 1983b K85 - Kaler 1985 K88 - Kaler 1988 KAC76 - Kaler et al. 1976b KFL88 - Kinman et al. 1988 KH81 - Kaler & Hartkopf 1981 KJ89 - Kaler & Jacoby 1989 KJ91 - Kaler & Jacoby 1991 KL85 - Kaler & Lutz 1985 KM81 - Kohoutek & Martin 1981 KPK87 - Kaler et al. 1987 KSK90 - Kaler et al. 1990 LFR91 - Lopez et al. 1991 PRM89 - Pena et al. 1989 PTP71 - Peimbert & Torres-Peimbert 1971 PTP87 - Peimbert & Torres-Peimbert 1987 RPD91 - Ratag et al. 1991 SB87 - Shaw & Bidelman 1987 SFO84 - Sabbadin et al. 1984 SK89 - Shaw & Kaler 1989 TPP77 - Torres-Peimbert & Peimbert 1977 TPP79 - Torres-Peimbert & Peimbert 1979 TPP90 - Torres-Peimbert et al. 1990 TS87 - Tamura & Shaw 1987 W88 - Webster 1988 --- l_Halpha Limit flag for Halpha intensity --- Halpha intensity of the Halpha line on the scale Hbeta=100 --- u_Halpha Uncertainty flag on Halpha intensity --- r_Halpha Short references for Halpha (full references in the paper) number=1 References to Table 1 are: A78 - Ahern 1978 AC79 - Aller & Czyzak 1979 AC83 - Aller & Czyzak 1983 AK87 - Aller & Keyes 1987 AS - Acker-Stenholm survey ASH84 - Adams et al. 1984 B78 - Barker 1978 B80 - Barker 1980 B86 - Barker 1986 B88 - Barker 1988 BC84 - Barker & Cudworth 1984 CPT87 - Clegg et al. 1987 CSP83 - Clegg et al. 1983 CRB91 - McCarthy et al. 1991 DHT90 - Dopita et al. 1990 FP91 - de Freitas Pacheco et al. 1991 FP92 - de Freitas Pacheco et al. 1992 GMC85 - Gutierrez-Moreno et al. 1985 HM78 - Hawley & Miller 1978 K76 - Kaler 1976a K76b - Kaler 1976b K80 - Kaler 1980 K83a - Kaler 1983a K83b - Kaler 1983b K85 - Kaler 1985 K88 - Kaler 1988 KAC76 - Kaler et al. 1976b KFL88 - Kinman et al. 1988 KH81 - Kaler & Hartkopf 1981 KJ89 - Kaler & Jacoby 1989 KJ91 - Kaler & Jacoby 1991 KL85 - Kaler & Lutz 1985 KM81 - Kohoutek & Martin 1981 KPK87 - Kaler et al. 1987 KSK90 - Kaler et al. 1990 LFR91 - Lopez et al. 1991 PRM89 - Pena et al. 1989 PTP71 - Peimbert & Torres-Peimbert 1971 PTP87 - Peimbert & Torres-Peimbert 1987 RPD91 - Ratag et al. 1991 SB87 - Shaw & Bidelman 1987 SFO84 - Sabbadin et al. 1984 SK89 - Shaw & Kaler 1989 TPP77 - Torres-Peimbert & Peimbert 1977 TPP79 - Torres-Peimbert & Peimbert 1979 TPP90 - Torres-Peimbert et al. 1990 TS87 - Tamura & Shaw 1987 W88 - Webster 1988 --- Patricia Bauer CDS 1994 May 03 J_A+AS_106_559.xml Deep CCD BV photometry of the poorly studied open cluster NGC 4815 J/A+AS/106/573 J/A+AS/106/573 NGC4815 BV photometry Deep CCD BV photometry of the poorly studied open cluster NGC 4815 G Carraro S Ortolani Astron. Astrophys. Suppl. Ser. 106 573 1994 1994A&AS..106..573C Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 4815) stars: luminosity function, mass function We report BV Johnson CCD photometry of 2498 stars in the region of the poorly studied open cluster NGC 4815. This object appears in the Janes (1988) list of possible old open clusters. NGC 4815 lies in the galactic plane, in a region of strong absorption. The color magnitude diagram (CMD) we derive shows that NGC 4815 has about the Hyades age (5x10^8^yr) and a probable lower than solar metal abundance. The color excess E_B-V_ and the distance modulus (m-M) turn out to be 0.70 and 14.10, respectively. Accordingly a distance of 2.5 Kpc from the Sun is derived. The luminosity function (LF) we obtain for the main sequence (MS) stars is consistent with a Salpeter (x=1.55) initial mass function (IMF).
Photometric data for NGC 4815 N Identification number --- X X coordinate --- Y Y coordinate --- V V magnitude mag B-V B-V color mag e_B-V rms uncertainty on B-V mag Patricia Bauer CDS 1994 Apr 22 J_A+AS_106_573.xml A new frequency analysis of photometric observations of the beta Cephei star IL Velorum J/A+AS/106/79 J/A+AS/106/79 A new frequency anaylsis of photometric observ A new frequency analysis of photometric observations of the beta Cephei star IL Velorum D Heynderickx U Haug Astron. Astrophys. Suppl. Ser. 106 79 1994 1994A&AS..106...79H Stars, early-type Stars, variable stars: early-type stars: individual (IL Vel) stars: oscillations stars: variables: other We present a new frequency-analysis of Johnson UBV-data of the {beta} Cephei star IL Vel, obtained between 1977 and 1979. This new analysis was inspired by more recent measurements of IL Vel in the Walraven five-colour photometric system. These data suggested the presence of frequencies not found in the original analysis of the UBV-data. From the new analysis, we conclude that four frequencies can be identified with certainty in the variations of IL Vel: f_0_=5.464973+/-0.000005, f_1_=5.363229+/-0.000006, f_2_=5.48838+/-0.00002 and f_3_=5.44184+/-0.00003, in cycles per day. The frequencies f_0_, f_2_ and f_3_ form a closely spaced triplet.
Walraven VBLUW photometry of HD80383 HJD Heliocentric Julian Day d Vw Walraven V, log(intensity) mag (V-B)w Walraven V-B, log(intensity) mag (B-U)w Walraven B-U, log(intensity) mag (U-W)w Walraven U-W, log(intensity) mag (B-L)w Walraven B-L, log(intensity) mag Johnson UBV photometry of HD80383 HJD Heliocentric Julian Day d V Johnson V mag B Johnson B mag U Johnson U mag Patricia Bauer CDS 1994 Mar 23 J_A+AS_106_79.xml Photographic observations of visual double stars J/A+AS/107/235 J/A+AS/107/235 Photographic observations of visual double stars Photographic observations of visual double stars D M D Jasinta E Soegiartini Astron. Astrophys. Suppl. Ser. 107 235 1994 1994A&AS..107..235J astrometry binaries: visual We present the analysis result of photographic observations of 221 visual double stars, observed in the years 1987-1989 with the 60-cm double-refractor at the Bosscha Observatory at Lembang, Java.
Photographic observations of visual double stars Photographic observations of visual double stars from Hipparcos programme RAh Right Ascension (1900) h RAm Right Ascension (1900) min RAm2000 Right Ascension (2000) min DE- Declination sign --- DEd Declination (1900) deg DEm Declination (1900) arcmin DEm2000 Declination (2000) arcmin Star Star name --- Mag1 First component magnitude mag n_Mag1 Separation sign --- Mag2 Second component magnitude mag Spect Spectra of the components --- Epoch Mean epoch of observations yr SepRA Mean value of D{alpha}cos{delta} arcsec e_SepRA Standard error on D{alpha}cos{delta} mas SepDE Mean value of D{delta} arcsec e_SepDE Standard error on D{delta} mas Rho Angular distance arcsec e_Rho Standard error in angular distance mas Theta Position angle deg e_Theta Standard error in position angle 10-2deg Plates Number of plates --- Images Number of images --- Weight Weight 10-3 Notes Notes --- Simona Mei CDS 1995 Jul 28 J_A+AS_107_235.xml Photometric CCD sequences in 7 southern Abell clusters J/A+AS/107/277 J/A+AS/107/277 CCD photometry of Abell clusters Photometric CCD sequences in 7 southern Abell clusters B Cunow W F Wargau Astron. Astrophys. Suppl. Ser. 107 277 1994 1994A&AS..107..277C galaxies: clusters: general galaxies: photometry techniques: photometric Photometric CCD sequences obtained in the fields of 7 southern Abell clusters are presented. The catalogue contains V and R magnitudes for 87 galaxies and 96 stars with 13<V<22.
VR magnitudes of 10 galaxies and 8 stars with 13 < V < 22 in the fields of the southern Abell cluster 2841, ESO/SERC field no. 195 VR magnitudes of 7 galaxies and 14 stars with 13 < V < 22 in the fields of the southern Abell cluster S0191, ESO/SERC field no. 030 VR magnitudes of 7 galaxies and 19 stars with 13 < V < 22 in the fields of the southern Abell cluster 3103, ESO/SERC field no. 054 VR magnitudes of 18 galaxies and 12 stars with 13 < V < 22 in the fields of the southern Abell cluster O0495, ESO/SERC field no. 484 VR magnitudes of 15 galaxies and 13 stars with 13 < V < 22 in the fields of the southern Abell cluster 3888, ESO/SERC field no. 345 VR magnitudes of 15 galaxies and 14 stars with 13 < V < 22 in the fields of the southern Abell cluster O2583, ESO/SERC field no. 605 VR magnitudes of 15 galaxies and 16 stars with 13 < V < 22 in the fields of the southern Abell cluster 4028, ESO/SERC field no. 110 No Object number --- Type Object type, S: star, G: galaxy --- RAh right ascension 2000 h RAm right ascension 2000 min RAs right ascension 2000 s DE- declination sign --- DEd declination 2000 deg DEm declination 2000 arcmin DEs declination 2000 arcsec V V magnitude mag R R magnitude mag V-R V-R colour mag Patricia Bauer CDS 1994 May 25 J_A+AS_107_277.xml A CCD survey of galaxies. III. Observations with the Loiano 1.5m telescope J/A+AS/107/285 J/A+AS/107/285 CCD survey of galaxies. III. A CCD survey of galaxies. III. Observations with the Loiano 1.5m telescope G Gavazzi I Randone Astron. Astrophys. Suppl. Ser. 107 285 1994 1994A&AS..107..285G galaxies: clusters: general galaxies: photometry Continuing a CCD survey of galaxies belonging or projected onto the Coma and Hercules Superclusters and to the A262, Virgo and Cancer clusters, we present isophote maps and photometric profiles in the Johnson system of 127 galaxies (126 taken in the V, 28 of which also in the B band, one only in B). For the objects in common we compare our results with those in the RC3.
Target galaxies CGCG CGCG denomination --- NGC NGC/IC denomination --- UGC UGC denomination --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec T Morphological type --- Memb Membership parameter --- m(pg) CGCG photographic magnitude mag a Major diameter arcmin b Minor diameter arcmin Vh Heliocentric galaxy velocity km/s Results of the present work CGCG CGCG denomination --- Filt Filter used --- Exp Exposure time min Date Observing date "DD/MM/YY" PQ Photometrical quality number=1 p means obtained during photometric conditions * indicates non photometric frames which were calibrated using aperture photometry available in the literature --- Seeing Seeing arcsec Sky Sky brightness mag/arcsec2 PA Position angle number=2 P.A. measured from north counterclockwise deg 1-b/a Ellipticity of elliptical rings --- a25 Observed radius along the major axis determined at the 25th magnitude isophote arcsec n_a25 An asterisk marks radii determined at the 24th magnitude isophote --- m25 Integrated magnitude at the 25th magnitude isophote mag n_m25 An asterisk marks magnitudes determined at the 24th magnitude isophote --- Patricia Bauer CDS 1994 May 19 Gavazzi G. J_A+AS_107_285.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest X: Ne VIII and Na IX J/A+AS/107/349 J/A+AS/107/349 Stark broadening X. Stark broadening of spectral lines of multicharged ions of astrophysical interest X: Ne VIII and Na IX M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 107 349 1994 1994A&AS..107..349D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar MgI lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles molecular data Using a semi classical approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 20 Ne VIII and 8 Na IX multiplets. Obtained results have been compared with available experimental and theoretical data. The influence of the perturber charge on the ion broadening contribution has been investigated and discussed.
Stark broadening parameters due to e-, p- and He III-impacts for Ne VIII and Na IX N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We Note on We number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de Note on de number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp Note on Wp number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- Wp FWHM for proton impacts (2) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp Note on dp number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dp shift for proton impacts (3) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ Note on WHe++ number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ Note on dHe++ number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dHe++ shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1994 May 26 Sylvie Sahal-Brechot & Milan S. Dimitrijevic J_A+AS_107_349.xml Elemental abundance studies of CP stars: The silicon star HD 43819 and the CP Star HD 147550 J/A+AS/107/353 J/A+AS/107/353 CP stars Elemental abundance studies of CP stars: The silicon star HD 43819 and the CP Star HD 147550 Z Lopez-Garcia S J Adelman Astron. Astrophys. Suppl. Ser. 107 353 1994 1994A&AS..107..353L stars: abundances stars: chemically peculiar stars: individual (HD 43819, HD 147550) Fine analyses of the silicon star HD 43819 and the CP star HD 147550 are presented using ATLAS9 model atmospheres whose predictions fit the optical region spectrophotometry and H{gamma} profiles and have the same bulk metallicity as the deduced abundances. For HD 43819 except for scandium and nickel, the derived abundances of the iron peak elements are around 10 times solar while those of the rare earths are about 1000 times solar. The lighter elements are generally underabundant except for silicon and calcium which are overabundant. HD 147550 is helium and calcium poor; carbon, magnesium, aluminum, scandium, titanium, and iron normal; and sulfur, chromium, manganese, nickel, strontium, zirconium, barium, europium, and mercury rich. It is a nonmagnetic CP star intermediate between the HgMn and the hot Am stars.
Elemental abundances Element Element --- No Multiplet Number --- Lambda Wavelength 0.1nm log(gf) Oscillator strength --- r_log(gf) Reference to oscillator strength number=1 Sources of gf-values: BK = Biemont et al. (1982A&A...107..166B) DW = Dworetsky (1972PASP...84..652D) GB = Grevesse et al. (1981, Upper Main Sequence CP Stars, 23rd. Liege Astrophys. Coll., 211) KX = Kurucz (1993, ASP Conf. Ser. 44, 87) LA = Lanz & Artru (1985PhyS...32..115L) MC = Magazzu & Cowley (1986ApJ...308..254M) MF = Martin, Fuhr & Wiese (1988, Cat. <VI/72>) for Sc through Mn; Fuhr, Martin & Wiese (1988, Cat. <VI/72>) for Fe through Ni; SC = Schaeffer (1971ApJ...163..411S) WD = Ward (1985MNRAS.213...71W) WF = Wiese & Fuhr (1975JPCRD...4..263W) WM = Wiese & Martin (1980, NSRDS-NBS 68, Part.2, US Governement Printing Office, Washington) WS= Wiese, Smith & Glennon (1966, NSRDS-NBS 4, US Governement Printing Office, Washington) and Wiese, Smith & Miles (1969) --- W1 Equivalent width for HD 43819 0.1pm log(N/Ntot)1 Deduced abundance for HD43189 number=2 N = number of atoms/volume of particular element Ntotal = number of atoms/volume of all elements --- W2 Equivalent width for HD 147550 0.1pm log(N/Ntot)2 Deduced abundance for HD 147550 number=2 N = number of atoms/volume of particular element Ntotal = number of atoms/volume of all elements --- Relative abundances Element Element --- log(El/Ntot)1 Elemental abundance for HD 43819 number=1 El = Element Ntot = number of atoms/volume of all elements --- u_log(El/Ntot)1 Uncertainty flag on log(El/Ntot)1 --- e_log(El/Ntot)1 rms uncertainty on log(El/Ntot)1 --- log(El/Ntot)2 Elemental abundance for HD 147550 number=1 El = Element Ntot = number of atoms/volume of all elements --- e_log(El/Ntot)2 rms uncertainty on log(El/Ntot)2 --- Patricia Bauer CDS 1994 May 19 J_A+AS_107_353.xml Broad band JHK infrared photometry of an extended sample of late type dwarfs and subdwarfs J/A+AS/107/365 J/A+AS/107/365 Dwarfs and subdwarfs IR photometry Broad band JHK infrared photometry of an extended sample of late type dwarfs and subdwarfs A Alonso S Arribas C Martinez-Roger Astron. Astrophys. Suppl. Ser. 107 365 1994 1994A&AS..107..365A infrared: stars stars: fundamental parameters stars: late-type stars: Population II subdwarfs The results of a long term programme of broad band JHK photometry, for a sample of 360 late type stars, made at the Observatorio del Teide (Tenerife, Spain) are presented.
Infrared photometric magnitudes measured at the Observatorio del Teide (TCS) ID Name --- Jmag J magnitude mag e_Jmag rms uncertainty on J mag Hmag H magnitude mag e_Hmag rms uncertainty on H mag Kmag K magnitude mag u_Kmag Uncertainty flag on K --- e_Kmag rms uncertainty on K mag o_Jmag Number of measurements for J, H and K --- Vmag V magnitude mag B-V B-V colour mag U-B U-B colour mag Com Comments number=1 References key: CL: Carney B.W. & Latham D.W. 1987, AJ 92, 116 SK: Sandage A. & Kowal C. 1986, AJ 91, 1140 SN: Schuster W.J. & Nissen P.E. 1989, A&A 221, 65 and A&A 222, 69 Par: Parallax subprogramme SH: Stauffer J.R. & Hartmann L.W. 1986, ApJSS 61, 531 B90: Beers T.C. et al. 1990, AJ 100, 849 RN: Ryan S.G. & Norris J.E. 1991, AJ, 101, 1835 Cay: Cayrel de Strobel G. et al. 1992, A&AS 95, 273 by: Stroemgren Photometry beta: beta photometry RI: RI photometry DwM: dwarf M Fstd: Faint standard This column also contains the spectral type and the number from hd, bd OR LTT catalogues. Individual notes: G026-012: K not measured at TCS has been assigned with Carney 1983 (AJ 88, 610), given the good agreement for J and H. G033-009: (V-K) too large, probable misidentification. G036-050: The two measurements in J differ in 0.2 mag. G106-049: Variable, {DELTA}J=0.2, {DELTA}H=0.16, {DELTA}K=0.13. G124-023: Misidentification. G208-029: Variable? HD128959: The two measurements in J differ in 0.16 mag. HD188510: Only one measurement in K. HD74000 : Unknown star measured instead HD74000. HD227638: Unknown star measured in the same field J=8.425 +/-0.035 , H=7.810 +/-0.014 , K=7.690 +/-0.014. HD229274: Variable? --- Infrared photometric magnitudes of the calibrating stars BS BS number --- n_BS Individual notes number=1 1: The fiducial J value for this star in Kidger 1992 is 4.839+/-0.018 with 8 re ported measurements. 2: The fiducial K value for this star in Kidger 1992 is 2.252+/-0.009 with 26 reported measurements. 3: The fiducial J,H and K values for this star in Kidger 1992 are, respectively , 4.043+/-0.013, 3.432+/-0.013 and 3.303+/-013 with 15 reported measurements. Reference: Kidger M. 1992, Carlos Sanchez Telescope Technical note series, Supplement to technical note #16, Calibration star programme results. --- Jmag J magnitude mag e_Jmag rms uncertainty on J mag Hmag H magnitude mag e_Hmag rms uncertainty om H mag Kmag K magnitude mag e_Kmag rms uncertainty on Kmag mag o_Jmag Number of measurements for J, H and K --- TSC p: primary standard of the TCS system s: secondary standard of the TCS system --- Sp Spectral type --- Infrared photometric extinction coefficients Date Observation date --- E(J) Extinction in J mag E(H) Extinction in H mag E(K) Extinction in K mag Com Comments number=1 f: full night, m: half night, p: less than half night, h: variable humidity, d: dust. --- Infrared photometric system of TCS Normalized filter transmissions JLam Wavelength in J band 0.1nm T(JLam) Normalized filter transmission in J band number=1 The sensitivity of the InSb detector has been included in normalized filter transmissions --- HLam Wavelength in H band 0.1nm T(HLam) Normalized filter transmission in H band number=1 The sensitivity of the InSb detector has been included in normalized filter transmissions --- KLam Wavelength in K band 0.1nm T(KLam) Normalized filter transmission in K band number=1 The sensitivity of the InSb detector has been included in normalized filter transmissions --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1994 Oct 13 J_A+AS_107_365.xml The Spacelab-1 Very Wide Field Survey of UV-excess objects. IV. The performance of the instrument in combination with optical photometry as a means of identifying stars with peculiar properties J/A+AS/107/385 J/A+AS/107/385 UV-excess objects Spacelab-1 survey IV. The Spacelab-1 Very Wide Field Survey of UV-excess objects. IV. The performance of the instrument in combination with optical photometry as a means of identifying stars with peculiar properties W Tobin M Viton J -P Sivan Astron. Astrophys. Suppl. Ser. 107 385 1994 1994A&AS..107..385T Galaxy: stellar content stars: fundamental parameters surveys ultraviolet: stars UV (195 nm) and Stroemgren uvby photometry of a 110 square degree field at high southern galactic latitudes are analyzed through a comparison of i) UV magnitudes for 57 stars of various types common to the published TD1 catalogue and the Very Wide Field Camera (VWFC); and ii) observed and theoretical two-colour diagrams. The higher sensitivity of the VWFC (=~0.5magnitude) and its more complete survey are exemplified by the detection and UV measurement of a series of objects with moderate UV-excess in addition to detection of some very blue objects of various nature down to fainter than 12th magnitude in the optical domain. A deeper survey with a VWFC-type instrument could provide a complete sample for studies of the group properties of faint blue stars. During the uvby reductions it was found that the usual procedure of plotting residuals as functions of declination, hour angle and airmass can be a powerful and diagnostic test of photometer rigidity.
Ultraviolet and Vuvby photometry for the completely-surveyed region indicated in Fig. 2 Vuvby photometry for other stars WT WT number --- Name Star name --- y/V Johnson V magnitude obtained by transformation of observations obtained with the Stroemgren y filter --- u_y/V Uncertainty flag on y/V --- e_y/V Internal error on y/V number=1 Single-star internal errors are reported for those stars for which any Stroemgren index exceeds 2.5 times the appropriate mean uncertainty reported in Table II --- (b-y) (b-y) colour mag e_(b-y) Internal error on (b-y) number=1 Single-star internal errors are reported for those stars for which any Stroemgren index exceeds 2.5 times the appropriate mean uncertainty reported in Table II mag m1 m1 colour index mag e_m1 Internal error on m1 number=1 Single-star internal errors are reported for those stars for which any Stroemgren index exceeds 2.5 times the appropriate mean uncertainty reported in Table II mag c1 c1 colour index mag e_c1 Internal error on c1 number=1 Single-star internal errors are reported for those stars for which any Stroemgren index exceeds 2.5 times the appropriate mean uncertainty reported in Table II mag nObs Number of observations --- m195 UV (195 nm) magnitude mag e_m195 rms uncertainty on m195 number=2 The error given to m_195_ magnitudes is twice the one derived by the CAPELLA software, see Viton et al (1991) mag n_e_m195 Note on e_m195 number=3 a uncertain error bar b VWFC image elongated, both HD 204779 and 204763 may contribute c CORAVEL data indicate possibly variable velocity d CORAVEL data indicate variable velocity e UV detection in fact due to WT026bis (Fig. 3, V=~12.5) which preliminary spectroscopy and CCD photometry has shown is a sdO star probably in binary association with a cooler companion f SAO 227683 excluded g SAO 227683 included h photometric and spectroscopic variable, suspected EB (see Prevot et al., 1993) + see Fig. 3 for finding .chart * see Viton et al. (1991) --- Com. Comments number=3 a uncertain error bar b VWFC image elongated, both HD 204779 and 204763 may contribute c CORAVEL data indicate possibly variable velocity d CORAVEL data indicate variable velocity e UV detection in fact due to WT026bis (Fig. 3, V=~12.5) which preliminary spectroscopy and CCD photometry has shown is a sdO star probably in binary association with a cooler companion f SAO 227683 excluded g SAO 227683 included h photometric and spectroscopic variable, suspected EB (see Prevot et al., 1993) + see Fig. 3 for finding .chart * see Viton et al. (1991) --- table1.tex LaTeX version of table1 table4.tex LaTeX version of table4 Patricia Bauer CDS 1994 May 25 J_A+AS_107_385.xml Correlated long-term light, colour and spectral variations of the Be star Kappa Dra J/A+AS/107/403 J/A+AS/107/403 Kappa Dra Correlated long-term light, colour and spectral variations of the Be star Kappa Dra K Juza P Harmanec H Bozic K Pavlovski J Ziznovsky A E Tarasov J Horn P Koubsky Astron. Astrophys. Suppl. Ser. 107 403 1994 1994A&AS..107..403J binaries: spectroscopic stars: emission-line, Be stars: variables: other Intensity of the Balmer emission lines of {kappa} Dra, documented by spectral records from the past 100 years, was found to vary with a period of 8406d (23.01yr). Optical brightness and continuum polarimetry seem to vary with the same period. Polarimetric changes are in phase with the emission strength. The brightness of the object attains maximum during the rise of emission. Then it declines to a local minimum which coincides with the maximum strength of the Balmer emission. Possible qualitative interpretation of these facts is briefly outlined.
List of comparison and check stars HR HR denomination --- HD HD denomination --- BD BD denomination --- Rem Remarks --- V V magnitude mag B-V B-V colour mag U-B U-B colour mag Sp Spectral type --- Seasonal means of UBV observations of Kappa Dra Season Observation date d Nobs Number of individual observations in given season --- V V magnitude mag B B magnitude mag U U magnitude mag B-V B-V colour mag U-B U-B colour mag Nightly means of UBV observations of Kappa Dra Published photometry of Kappa Dra HJD Mean heliocentric Julian date of observation d Nobs number of individual observations (table3) --- V V magnitude mag B B magnitude mag U U magnitude mag B-V B-V colour mag U-B U-B colour mag Ref References (table4) number=1 A: Mendoza E.E. 1958, ApJ 128, 207 B: Haeggkvist L. & Oja T. 1966, Ark. Astron. 4, 137 C: Johnson H.L. et al. 1966, Comm. Lun. Planet. Lab. 4, 99 D: Burki D.G. 1980, Geneva photometry of Be stars, priv. comm. E: Papousek J. 1979, Scripta Fac. Sci. Nat. Univ. Purkynianae Brunensis Phys. 9, 75 F: Dapergolas A. et al. 1981, Inf. Bull. Var. Stars No. 1920 G: Schuster W.J. & Alvarez M. 1983, PASP 95, 35 H: Johnson H.L. & Mitchell R.I. 1969, Comm. Lun. Planet. Lab. 8, 1 I: Gulliver A.F. 1983, priv. comm. J: Alvarez M. & Schuster W.J. 1982, Rev. Mex. Astron. Astrofis. 5, 173 K: Schuster W.J. & Guichard J. 1984, Rev. Mex. Astron. Astrofis. 9, 141 L: Catalano S. & Umana G. 1987, Physics of the Be stars, IAU Colloq. N0. 92, 101 and private communication M: Haeggkvist L. 1971, A&A 12, 5 Symbols * and + attached to the authors code in the last column denote original measurements in other photometric systems than UBV, and publication of only mean values of individual measurements, respectively. No exact times of observations were given in papers A, B, G, H and M. --- Equivalent width of H alpha Published equivalent width of H alpha HJD Mean heliocentric Julian date of observation d EW Equivalent width of Halpha line --- Source Source (see note (1) of table5b) --- Strength of emission of H beta Published strength of emission of H beta HJD Mean heliocentric Julian date of observation d E/C Strength of Hbeta emission --- Source Source number=1 O : photographic spectrograms from Ondrejov OR: Reticon spectrograms from Ondrejov R : photographic spectrograms from Rozen CD: CCD spectrograms from Crimea A : Underhill A.B. 1953, MNRAS 113, 477 B : Bahng J.D.R. 1976, Be and Shell Stars, IAU Symposium No. 70, ed. A. Slettebak (D. Reidel, Dordrecht) 41 C : Lacy C.H. 1977, ApJ 212, 132 D : Slettebak A. & Reynolds R.C. 1978, ApJ 38, 205 E : Reynolds R.C. & Slettebak A. 1980, PASP 92, 472 F : Andrillat Y. & Fehrenbach C. 1981, Workshop On Pulsating Be Stars eds. G.E.V.O.N. and C. Sterken (Nice Observatory Publ.) 255 G : Ghosh K.K. 1990, ApJS 72, 543 H : Curtiss R.H. 1932, Publ. Astron. Obs. Univ. Michigan 4, No. 12, 163 I : Jessup M.K. 1932, ApJ 76, 75 --- Patricia Bauer CDS 1994 Oct 18 J_A+AS_107_403.xml Circumstellar dust envelopes of oxygen-rich AGB stars J/A+AS/107/445 J/A+AS/107/445 Envelopes of oxygen-rich AGB stars Circumstellar dust envelopes of oxygen-rich AGB stars O Hashimoto Astron. Astrophys. Suppl. Ser. 107 445 1994 1994A&AS..107..445H circumstellar matter infrared: stars stars: AGB and post-AGB stars: mass-loss Using IRAS observational data, the best-fitting models are searched for oxygen-rich AGB stars in various evolutionary stages from optically visible red giant stars to OH/IR stars with heavy mass loss. The model infrared spectral energy distributions of the red giant stars with circumstellar dust envelopes are calculated with the use of a radiative transfer code. It is found that the oxygen-rich IRAS AGB stars surrounded by circumstellar dust envelopes are divided into three groups, which can be clearly distinguished by their mass loss rate and the grain temperature at the inner boundary of the circumstellar dust envelopes. One group corresponds to Mira type objects with a moderate mass loss rate and a grain formation temperature of about 500 K, the second to OH/IR star type objects with a large mass loss rate and a high grain formation temperature, and the third to M stars with a very cold grain temperature at the inner boundary, indicating that the moderate mass loss stopped a considerable time ago in these objects. The higher grain formation temperature of the OH/IR star type objects indicates a grain formation point closer to the stellar surface, suggesting an effective acceleration of dust grains by radiation pressure. Such an effective acceleration can play an important role in the mass loss phenomena of OH/IR stars with large mass loss rates. From the model fitting results, it is suggested that an AGB star undergoes several dozen phases of moderate mass loss of {dot}(M)~10^-7^-10^-6^M_{sun}_/yr for a period of 10^3^-10^4^years with interruptions of 10^3^-10^4^years during the ordinary Mira variable phase before becoming an OH/IR star with a mass loss rate exceeding 10^-5^M_{sun}_/yr and a lifetime of about 10^3^-10^4^years.
Best fit model parameters for IRAS 2n and 3n sources Best fit model parameters for the IRAS red 1n M stars IRAS IRAS name --- Id. Identification --- T* Stellar temperature K ri/r* Inner boundary of the dust envelope in stellar radius --- ro/r* Outer boundary of the dust envelope in stellar radius --- log(n0) Number density parameter cm-3 Td(ri) Grain temperature at ri K chi2 Fitting error --- c1I log(S25/S12) of IRAS data --- c2I log(S60/S25) of IRAS data --- 10umI 10 micron band feature -in IRAS LRS spectrum for table1 -of IRAS data ( = 0.0 ) for table2 --- c1M log(S25/S12) of the model --- c2M log(S60/S25) of the model --- 10umM 10 micron band feature of the model --- table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 Patricia Bauer CDS 1994 Jun 02 J_A+AS_107_445.xml Position of Uranian satellites J/A+AS/107/559 J/A+AS/107/559 Position of Uranian satellites Position of Uranian satellites C H Veiga R Vieira Martins Astron. Astrophys. Suppl. Ser. 107 559 1994 1994A&AS..107..559V astrometry planets and satellites: individual (satellites of Uranus) Positions of Uranian satellites from 333 photographic plates obtained at the Cassegrain focus of a 1.6 m reflector are given for the oppositions of 1983 through 1988. These positions were reduced using photometric methods and compared with those calculated theoretically calculated from GUST86. The observed minus calculated residuals referred to Oberon, have standard deviations of the order of 0".04 for the four greatest Uranian satellites and 0".09 for Miranda. These residuals for the four satellites are better than the most precise found in the literature.
Observed positions of the Uranian satellites Np plate number --- Obsy Observing date UTC (year) yr Obsm Observing date UTC (month) --- Obsd Observing date UTC (day) d Ns Satellite number number=1 Satellite number: 5: Miranda, 1: Ariel, 2: Umbriel, 3: Titania --- X X = DELTA(alpha)cos(delta); equatorial coordinate 1950.0 referred to Oberon arcsec Y Y = DELTA(delta); equatorial coordinate 1950.0 referred to Oberon arcsec Patricia Bauer CDS 1994 Jun 03 J_A+AS_107_559.xml Photometric and spectroscopic observations of the spotted T Tauri star V410 Tauri J/A+AS/107/9 J/A+AS/107/9 V410 Tau Photometric and spectroscopic observations of the spotted T Tauri star V410 Tauri P P Petrov V A Shcherbakov S V Berdyugina V S Shevchenko K N Grankin S Y Melnikov Astron. Astrophys. Suppl. Ser. 107 9 1994 1994A&AS..107....9P stars: imaging stars: individual (V410 Tau) stars: pre-main sequence V410 Tau is a fast rotating weak line T Tau star with a large cool spot or spotted area on its surface, which has been observed through the periodic (P=1.872d) light variations during several years. We present here UBVR photometric monitoring data for the star for 7 years since 1986 to 1992. The data permit us to derive the spot parameters and search for their annual variations. In 1992/93 the photometric monitoring was carried out along with low resolution high signal-to-noise spectroscopy of V410 Tau in the spectral region of the TiO bands near {lambda}7100, Li I{lambda}6707 and H{alpha}. We found a relationship between the TiO bands strength and stellar brightness in favor of the cool spot hypothesis. Parameters of the spotted region were derived, and an integrated spectrum of the spotted star was calculated using synthetic spectra of stellar atmospheres. The H{alpha} emission was found to vary in a more complex way, with two flux maxima at the phases of axial rotation when the spot is near the stellar limb. High resolution H{alpha} profiles were obtained for all phases of the rotational period.
UBVRI photometry of V410 Tau in 1986-1992 JD Julian day d V V magnitude mag U-B U-B colour mag B-V B-V colour mag V-R V-R colour mag Patricia Bauer CDS 1994 May 06 J_A+AS_107_9.xml CCD photometry of distant open clusters: I. Berkeley 22, Berkeley 29 and Berkeley 54 J/A+AS/108/151 J/A+AS/108/151 Open clusters CCD photometry. I. CCD photometry of distant open clusters: I. Berkeley 22, Berkeley 29 and Berkeley 54 J Kaluzny Astron. Astrophys. Suppl. Ser. 108 151 1994 1994A&AS..108..151K blue stragglers Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Be 22, Be 29, Be 54) We present deep BVI photometry for three previously unstudied rich and distant open clusters. The color-magnitude diagrams of all studied objects show well-defined main-sequences and clumps of helium burning giants. Estimates of age, reddening and distance are given for all target clusters. Ages of Be 54 and Be 29 are close to the age of M 67 (about 4Gyr on the scale of Geneva isochrones). Age of Be 22 is about 3Gyr. Heliocentric distance of Be 29 is estimated at 10.5 kpc while its galactocentric distance is about 19kpc. Be 29 seems to be the most distant galactic open cluster known in sense of its heliocentric as well as galactocentric distance. A clearly marked sequence of binaries is visible on the color-magnitude diagram of Be 29. Two likely candidates for evolved giants belonging to the very extended halo of Be 29 were identified. Our photometry suggests extremely low metallicity of Be 29. Several candidates for variable stars were found in the field of Be 54.
VI photometry of stars from Be 54 field BVI photometry of stars from Be 22 field BVI photometry of stars from Be 29 field BV photometry of stars from Be 29 field (Las Campanas data) ID ID number --- X X coordinate, X axis points toward South number=1 1 pixel=0.30 arcsec pix X Y coordinate, Y axis points toward East number=1 1 pixel=0.30 arcsec pix Vmag V magnitude mag e_Vmag rms uncertainty on V mag o_Vmag Number of averaged V measurements --- q_Vmag Quality flag for V number=2 q=1 means relatively poor quality --- B-V B-V colour number=3 For table2 and table3, no value means "unknown color" mag e_B-V rms uncertainty on B-V mag o_B-V Number of averaged B measurements --- q_B-V Quality flag for B-V number=2 q=1 means relatively poor quality --- V-I V-I colour number=3 For table2 and table3, no value means "unknown color" mag e_V-I rms uncertainty on V-I mag o_V-I Number of averaged I measurements --- q_V-I Quality flag for V-I --- Patricia Bauer CDS 1994 Sep 26 J_A+AS_108_151.xml Atomic data from the IRON Project. V. Effective collision strengths for transitions in the ground configuration of oxygen-like ions J/A+AS/108/1 J/A+AS/108/1 IRON Project. V. O-like ions Atomic data from the IRON Project. V. Effective collision strengths for transitions in the ground configuration of oxygen-like ions K Butler C J Zeippen Astron. Astrophys. Suppl. Ser. 108 1 1994 1994A&AS..108....1B J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data infrared: ISM: lines and bands plasmas Fine-structure collision strengths for transitions between the ground configuration terms of oxygen-like ions have been obtained in a six state close-coupling approximation. Effective collision strengths are tabulated in the range of 1000-100000K for the following ions: F II, Ne III, Na IV, Mg V, Al VI, Si VII, P VIII, S IX, Cl X, Ar XI.
Observed and calculated F II, Ne III and Na IV target ion energies Observed and calculated Mg V, Al VI and Si VII target ion energies Observed and calculated P VIII, S IX and Cl X target ion energies Observed and calculated Ar XI target ion energies El. Element --- Tr. Transition --- Obs Observed target ion energy cm-1 Cal Calculed target ion energy cm-1 Effective collision strengths for F II Effective collision strengths for Ne III Effective collision strengths for Na IV Effective collision strengths for Mg V Effective collision strengths for Al VI Effective collision strengths for Si VII Effective collision strengths for P VIII Effective collision strengths for S IX Effective collision strengths for Cl X Effective collision strengths for Ar XI logT Temperature K Gamma1 effective collision strength for transition ^3^P_0_-^3^P_1_ --- Gamma2 effective collision strength for transition ^3^P_0_-^3^P_2_ --- Gamma3 effective collision strength for transition ^3^P_1_-^3^P_2_ --- Gamma4 effective collision strength for transition ^3^P_0_-^1^D --- Gamma5 effective collision strength for transition ^3^P_1_- ^1^D --- Gamma6 effective collision strength for transition ^3^P_2_-^1^D --- Gamma7 effective collision strength for transition ^3^P_0_-^1^S --- Gamma8 effective collision strength for transition ^3^P_1_-^1^S --- Gamma9 effective collision strength for transition ^3^P_2_-^1^S --- Gamma10 effective collision strength for transition ^1^D-^1^S --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1994 Jun 16 J_A+AS_108_1.xml Fundamental parameters of Cepheids: II. Radial velocity data J/A+AS/108/25 J/A+AS/108/25 Cepheids fundamental parameters II. Fundamental parameters of Cepheids: II. Radial velocity data D Bersier G Burki M Mayor A Duquennoy Astron. Astrophys. Suppl. Ser. 108 25 1994 1994A&AS..108...25B Cepheids stars: individual (DL Cas, W Sgr) stars: oscillations Radial velocity data for 40 Cepheid stars obtained with the CORAVEL spectrometer are presented. They represent 1203 individual observations. The mean number of measurements per star is 41, ranging from 10 to 133. For each star, a Fourier analysis has been made and we searched the period that gave the best fit for the velocity curve. When the data covered a sufficiently long time interval, it has been looked for period changes or phase jumps. The results have been compared to those found in the literature; the choice of the best periods is discussed, taking into consideration the uncertainty on the period, the smoothness of the fit and several other parameters. New orbital elements, based on CORAVEL measurements only, are given for DL Cas and W Sgr.
Radial velocities for 40 Cepheids Name Star name --- HD HD number or BD number or coordinates 1900 --- JD Date of measurement in Julian day d RV Radial velocity km/s e_RV Rms uncertainty on the radial velocity km/s Fourier coefficients of the radial velocity curves Name Name --- Freq. Frequency d-1 A0 Amplitude A0 km/s n_A0 A ) indicates that for the binaries and suspected binaries, the center-of-mass velocity has been set to zero --- eps(fit) standard deviation around the fit km/s T0 epoch (HJD) d A1 amplitude of the harmonic Freq. km/s L1 Lanczos coefficient --- phi1 phase of Freq. rad A2 amplitude of the harmonic 2*Freq. km/s L2 Lanczos coefficient --- phi2 phase of the harmonic 2*Freq. rad A3 amplitude of the harmonic 3*Freq. km/s L3 Lanczos coefficient --- phi3 phase of the harmonic 3*Freq. rad A4 amplitude of the harmonic 4*Freq. km/s L4 Lanczos coefficient --- phi4 phase of the harmonic 4*Freq. rad A5 amplitude of the harmonic 5*Freq. km/s L5 Lanczos coefficient --- phi5 phase of the harmonic 5*Freq. rad A6 amplitude of the harmonic 6*Freq. km/s L6 Lanczos coefficient --- phi6 phase of the harmonic 6*Freq. rad A7 amplitude of the harmonic 7*Freq. km/s L7 Lanczos coefficient --- phi7 phase of the harmonic 7*Freq. rad A8 amplitude of the harmonic 8*Freq. km/s L8 Lanczos coefficient --- phi8 phase of the harmonic 8*Freq. rad A9 amplitude of the harmonic 9*Freq. km/s L9 Lanczos coefficient --- phi9 phase of the harmonic 9*Freq. rad A10 amplitude of the harmonic 10*Freq. km/s L10 Lanczos coefficient --- phi10 phase of the harmonic 10*Freq. rad A11 amplitude of the harmonic 11*Freq. km/s L11 Lanczos coefficient --- phi11 phase of the harmonic 11*Freq. rad A12 amplitude of the harmonic 12*Freq. km/s L12 Lanczos coefficient --- phi12 phase of the harmonic 12*Freq. rad A13 amplitude of the harmonic 13*Freq. km/s L13 Lanczos coefficient --- phi13 phase of the harmonic 13*Freq. rad A14 amplitude of the harmonic 14*Freq. km/s L14 Lanczos coefficient --- phi14 phase of the harmonic 14*Freq. rad A15 amplitude of the harmonic 15*Freq. km/s L15 Lanczos coefficient --- phi15 phase of the harmonic 15*Freq. rad A16 amplitude of the harmonic 16*Freq. km/s L16 Lanczos coefficient --- phi16 phase of the harmonic 16*Freq. rad A17 amplitude of the harmonic 17*Freq. km/s L17 Lanczos coefficient --- phi17 phase of the harmonic 17*Freq. rad A18 amplitude of the harmonic 18*Freq. km/s L18 Lanczos coefficient --- phi18 phase of the harmonic 18*Freq. rad table3.tex LaTeX version of table3 Patricia Bauer CDS 1994 May 26 J_A+AS_108_25.xml Atomic data for absorption lines from the ground level at wavelengths greater than 228 A J/A+AS/108/287 J/A+AS/108/287 Atomic data Atomic data for absorption lines from the ground level at wavelengths greater than 228 A D A Verner P D Barthel D Tytler Astron. Astrophys. Suppl. Ser. 108 287 1994 1994A&AS..108..287V atomic data quasars: absorption lines ultraviolet: general We list wavelengths, statistical weigths and oscillator strengths for 2249 spectral lines arising from the ground states of atoms and ions. The compilation covers all wavelengths longward of the He II Lyman limit at 227. 838A and all the ion states of all elements from hydrogen to bismuth (Z=83) for which reliable data are known. We assign experimental wavelengths to 1086 lines which have oscillator strengths calculated in the Opacity Project, and add 1163 lines which have critically evaluated oscillator strengths from previous compilations. The presented data are to be used for quasar absorption spectra interpretation. We use solar abundances to calculate the expected relative strengths of all absorption lines, and list separately the strongest lines above 228A expected in QSO absorption systems, many of which are listed here for the first time. The great majority of strong lines expected in quasar spectra are at {lambda}<912A. We also list the strongest absorption lines of various ions without wavelength restriction.
Strong lines above 228 A expected in quasar absorption systems lambda Wavelength 0.1nm Species Identification --- P Expected width (strength) parameter --- Strongest lines above 228 A without experimental wavelengths Species Identification --- Transition Transition --- Multiplet Multiplet --- lambda Theoretical wavelength 0.1nm Gi Lower level statistical weight --- Gk Upper level statistical weight --- Fik Oscillator strength --- P Expected width (strength) parameter --- Atomic weights and solar-system abundances Element Chemical element --- Z Atomic number --- Atomic weight Atomic weight --- Abundance Solar-system abundance --- Ionization thresholds and strongest lines of atoms and ions Species Identification --- Z Atomic number --- N Number of electrons --- Configuration Ground state electronic configuration. Only the five outer shells are indicated --- E Ionization potential eV lambda Vacuum wavelength 0.1nm Gi Lower level statistical weight --- Gk Upper level statistical weight --- Fik Oscillator strength --- P Expected width (strength) parameter number=1 P=log({lambda}f)+log(N/N_H_)+12.00 --- Resonance absorption lines above 228 A ordered by element Species Identification --- Z Atomic number --- N Number of electrons --- Transition Transition --- Multiplet Multiplet --- lambda Vacuum wavelength 0.1nm Gi Lower level statistical weight --- Gk Upper level statistical weight --- Fik Oscillator strength (Opacity Project) --- F'ik Oscillator strength (other sources) --- P Expected width (strength) parameter number=1 P=log({lambda}f)+log(N/N_H_)+12.00 --- Ref Reference to source of wavelength --- Resonance absorption lines above 228 A ordered by wavelength lambda Vacuum wavelength 0.1nm Species Identification --- Z Atomic number --- N Number of electrons --- Gi Lower level statistical weight --- Gk Upper level statistical weight --- Fik Oscillator strength --- P Expected width (strength) parameter number=1 P=log({lambda}f)+log(N/N_H_)+12.00 --- Patricia Bauer CDS 1994 Jul 01 Verner D.A. J_A+AS_108_287.xml High precision rotating neutron star models. II. Large sample of neutron stars properties J/A+AS/108/455 J/A+AS/108/455 Rotating neutron stars models. II. High precision rotating neutron star models. II. Large sample of neutron stars properties M Salgado S Bonazzola E Gourgoulhon P Haensel Astron. Astrophys. Suppl. Ser. 108 455 1994 1994A&AS..108..455S equation of state pulsars: general relativity stars: neutron stars: rotation A new and highly precise numerical approach for computing stationary rotating stellar configurations in general relativity has been employed to construct rotating neutron star models. Fourteen equations of state (EOS) of cold dense matter have been used to produce a "catalog" of thousands neutron star models, parametrized by the EOS, the central energy density and the angular velocity. The results are presented in a series of tables for each EOS. A particular emphasis is put on the properties of maximal mass models. These latter are useful to constrain the EOS, taking into account the observed pulsars.
Neutron star properties at fixed baryon mass for four equations of state (EOS). EOS EOS Equation of State used number=1 Equations of state Relativistiv models DiazII: Pure neutron matter, n-n interaction mediated via exchange of {sigma}, {pi}, {rho}, {omega} mesons. Ground state calculated by using renormalized Hartree approximation (Diaz Alonso 1985). HKP: Pure neutron matter, n-n interaction mediated via exchange of {sigma}, {omega}, {pi}, {rho} mesons. Calculating using an effective Lagrangian, done within the Hartree approximation. This particular model fits saturation density of nuclear matter n0-0.17fm^-3^ (Haensel et al. 1981). Glend1: "Case 1" model of Glendenning (1985). Baryon matter including nucleons, hyperons, {DELTA}s, and a pion condensate, in beta equilibrium with leptons. Strong interactions described by an effective Lagrangian, including couplings of baryons to {sigma}, {omega}, {pi}, {rho}, K mesons. Couplings of hyperons to meson fields reduced as compared to those of nucleons and {DELTA}s. Hartree approximation for the ground state. Glend2: "Case 2" model of Glendenning (1985). Similar to Glend1, but with no pion condensation because of an assumed repulsion between couplings of all baryons. Glend3: "Case 3" model of Glendenning (1985). Similar to Glend2, but with universal couplings of all baryons. WGW: For nb<0.3fm^-3^, neutron matter described using {LAMBDA}^00^ ladder approximation, with realistic Bonn meson-exchange interaction. For n>0.3fm^-3^, baryon matter described using relativistic Hartree approximation with effective Lagrangian, including couplings of nucleons and hyperons to {sigma}, {omega}, {pi}, {rho}, {eta}, {delta} mesons (Weber et al. 1991). Non-relativistic potential models PandN: Pure neutron matter. Interaction described by the Reid soft core potential. Ground state calculating using variational method (Pandharipande 1971). Causal at the densities encountered in neutron stars. BJ1: Baryon matter composed of nucleons, hyperons and {DELTA}s, in beta equilibrium with leptons. Baryon-baryon interaction described by the modified Reid soft core potential. Ground state calculated using variational method. This is model IH of Bethe & Johnson (1974) (see also Malone et al. 1975). Causal at the densities encountered in neutron stars. FP: Neutron matter, with nucleon-nucleon interaction described by a two-body Urbana UV_14_ potential, combined with a phenomenological three-neutron TNI interaction. Ground state of neutron matter calculated using variational method (Friedman & Pandharipande 1981). Non-causal at n>1fm^-3^. WFF(AV_14_+UVII): Nucleon matter in beta equilibrium with electrons and muons. Interaction described by a two-body Argonne AV_14_ potential, combined with phenomenological three-nucleon UVII interaction. Ground state of matter calculated in a very good approximation using sophisticated variational method (Wiringa et al., 1988). Non-causal at n>1.1fm^-3^ WFF(UV_14_+TNI): Nucleon matter in beta equilibrium with electrons and muons. Interaction described by a two-body Urbana UV_14_ potential, combined with a phenomenological three-nucleon TNI interaction. Ground state of matter calculated in a very good approximation using sophisticated variational method (Wiringa et al., 1988). Causal at the densities relevant for neutron stars. WFF(UV_14_+UVII): Nucleon matter in beta equilibrium with electrons and muons. Interaction described by a two-body Urbana UV_14_ potential, combined with a phenomenological three-nucleon UVII interaction. Ground state of matter calculated in a very good approximation using sophisticated variational method (Wiringa et al., 1988). Non-causal at n>1fm^-3^ Schematic analytic models Pol2: Polytrope p = {kappa}n^{gamma}, e=m_B_n+({kappa/({gamma}-1))n^{gamma} with {kappa}=1m_B_fm^3^ and {gamma}=2. Causal at all n. CLES: Causality-limit EOS. BJ1 model up to n=n*=0.3fm^-3^, continued by a schematic EOS p=e-e*+p*, where p*=p(n*), e*=e(n*) are given analytically (see Eq.3 of Haensel & Proszynski 1982). Maximally stiff while causal (velocity of sound = c) above n*. --- Hc Central pseudoenthalpy ---- Ec Central energy-density in Rho_nuc.c2 14.94x10+23kg/m/s2 Omega Rotational frequency 10+4s-1 P Period of rotation ms n_P A 'i' means infinity --- M Gravitational mass Sun Beta Baryon mass Sun Rcirc Circunferential (equatorial) radius km cJ/GM2 Angular momentum --- |1-lambda| Per cent error indicator --- tables.tex LaTeX version of tables Patricia Bauer CDS 1994 Jun 16 J_A+AS_108_455.xml On an alternative statistical distance scale for planetary nebulae. Catalog with statistical distances to planetary nebulae. J/A+AS/108/485 J/A+AS/108/485 PN distance scale On an alternative statistical distance scale for planetary nebulae. Catalog with statistical distances to planetary nebulae. G C M Van De Steene A A Zijlstra Astron. Astrophys. Suppl. Ser. 108 485 1994 1994A&AS..108..485V catalogs planetary nebulae: general We have proposed a statistical method to determine distances to planetary nebulae. The method is based on an empirical correlation between the radio-continuum brightness temperature and radius. Here we present a catalog of distance determinations calculated using this method.
Catalog of distances to planetary nebulae Name Nebula name --- PK PK number --- F5GHz Radio flux at 5 GHz mJy D Angular diameter arcsec Ref References number=1 (1) Pottasch S.R. 1984, "Planetary Nebulae" (Reidel, Dordrecht) (2) Aaquist A. & Kwok S. 1990, A&AS 84, 229 (3) Zijlstra A.A. et al. 1989, A&AS 79, 329 (4) Milne D.K. & Aller L.H. 1975, A&A, 38, 183 (5) Milne D.K. 1979, A&AS 36, 227 (6) Roelfsema P.R. et al. 1991, A&AS 79, 329 --- Tb Brightness temperature K R Radius calculated using the proposed method pc l_Dist Limit flag on distance --- Dist Distance calculated using the proposed method kpc tau(CKS) Optical thickness parameter --- log(mu) Ionised mass --- Rad(CKS) Radius as obtained with the Cahn et al. (CKS) calibration number=2 (CKS) Cahn J.H., Kaler J.B., Stanghellini L. 1992, A&AS 94, 399 pc Dist(CKS) Distance as obtained with the Cahn et al. (CKS) calibration number=2 (CKS) Cahn J.H., Kaler J.B., Stanghellini L. 1992, A&AS 94, 399 kpc Diff Difference between the distance determinations kpc Patricia Bauer CDS 1994 Jul 26 J_A+AS_108_485.xml The long-term behaviour of the photometric variability of Beta Cassiopeiae J/A+AS/108/55 J/A+AS/108/55 Beta Cas The long-term behaviour of the photometric variability of Beta Cassiopeiae E Riboni E Poretti G Galli Astron. Astrophys. Suppl. Ser. 108 55 1994 1994A&AS..108...55R delta Scuti methods: data analysis stars: individual (Beta Cas) stars: oscillations 1003 V measurements of {beta} Cas divided into three observing seasons are discussed. Their analysis performed with both the Vanicek least-squares and the classical O-C methods led us to the confirmation of the monoperiodic pulsation. All the photometry available on {beta} Cas (spanning 25 years) was also analyzed; the amplitude of the light curve was found to be constant, while a small period variability can be inferred.
Beta Cas V measurements HJD Heliocentric Julian day d Vmag V magnitude mag Patricia Bauer CDS 1994 Jun 14 J_A+AS_108_55.xml How did the spectrum of P Cygni look in 1985? Spectral atlas with complete line identifications in the wavelength range from 3550 to 4800A J/A+AS/108/561 J/A+AS/108/561 P Cygni spectrum in 1985 How did the spectrum of P Cygni look in 1985? Spectral atlas with complete line identifications in the wavelength range from 3550 to 4800A N Markova Astron. Astrophys. Suppl. Ser. 108 561 1994 1994A&AS..108..561M atlases line: identification stars: individual (P Cyg) stars: mass-loss Using the coude spectrograph of the NAO 2m RCC telescope at the Rodopa mountains, Bulgaria, nine spectra in the wavelength range from 3550 to 4800A of P Cygni were obtained during the year of 1985. By averaging these spectra we achieved a S/N -ratio of about 45. Here we present a spectral atlas with complete line identifications. Apart from the lines listed by de Groot (1969) many new lines of OII, NII and FeIII ions are identified. Few lines of NIII and SIII mainly from higher excitation levels are also observed. The most intensive lines of OIII and CIII are seen in absorption. In addition to the forbidden lines discovered by Stahl et al. (1991, 1993) a number of further forbidden lines are identified. A special feature of our spectrum is the appearance of AlIII lines in emission.
P Cygni spectrum - wavelengths and identifications LamObs Observational wavelengths 0.1nm u_LamObs '?' indicates an uncertain feature --- a/e Nature of the line: a = absorption, e = emission --- n_LamObs When two or more spectral features are believed to be formed by the same line or lines, the different features are connected by round brackets. --- LamLab Laboratory wavelengths 0.1nm Ion Ion identification --- n_Ion '*' marks the most important contributor to a blend --- Rem1 Remarks number=1 new = newly identified line 1 = line observed by de Groot (1969) 2 = line observed by Stahl et al. (1993) --- Rem2 Additional remarks number=2 IS = interstellar line bl = blend 1 = first absorption component 2 = second absorption component --- Overlap "--" marks the area of overlapping of forbidden and permitted line --- Forbidden Identification of forbidden lines --- Patricia Bauer CDS 1994 Jul 26 J_A+AS_108_561.xml Photometry of the young cluster NGC 330 in the Small Magellanic Cloud J/A+AS/108/571 J/A+AS/108/571 Photometry of the SMC cluster NGC 330 Photometry of the young cluster NGC 330 in the Small Magellanic Cloud A Vallenari S Ortolani C Chiosi Astron. Astrophys. Suppl. Ser. 108 571 1994 1994A&AS..108..571V globular clusters: individual (NGC 330) Hertzsprung-Russell (HR diagram) Magellanic Clouds techniques: photometric We present new Johnson BV CCD photometry of the young cluster NGC 330 in the Small Magellanic Cloud and of a nearby field. Comparing the surface brightness profile of the cluster with the density distribution models of Meylan (1987, 1988) and Elson (1991) we derive the structural parameters, namely the ellipticity, the concentration, and the core and tidal radii. The photometric quality and completeness of the data are analyzed in great detail to derive the reference Color-Magnitude Diagram (CMD) and the Luminosity Function (LF) for main sequence stars of the cluster.
BV CCD photometry of NGC 330 ID Identification number --- X X coordinate pix Y Y coordinate pix Vmag V magnitude mag B-V B-V colour mag e_Vmag rms uncertainty on Vmag mag Patricia Bauer CDS 1994 Aug 29 J_A+AS_108_571.xml The light variations of some CP2 SrCrEu J/A+AS/108/595 J/A+AS/108/595 CP2 SrCrEu stars light variation The light variations of some CP2 SrCrEu F A Catalano F Leone Astron. Astrophys. Suppl. Ser. 108 595 1994 1994A&AS..108..595C stars: chemically peculiar stars: variables: other In the framework of a programme of checking the periods of chemically peculiar stars, eight southern stars have been observed in the uvby system. Seven stars have been previously known to be light variables, but for some stars the periods were not accurate enough to phase together different kinds of observations carried out several years apart. The periods of HD 83368, HD 98088, and HD 153882 are confirmed. For the stars HD 49976, HD 111133, HD 118022, and HD 164258 we present here more refined values of the period. No variability has been detected for the star HD 137949 within a time scale of the order of ten days.
Observations Star1 Star name --- Star2 References star --- HJD Heliocentric julian day d n_HJD Data marked with an asterisk are not reported on Fig. 3 --- Du Magnitude difference (star1-star2) in u mag Dv Magnitude difference (star1-star2) in v mag Db Magnitude difference (star1-star2) in b mag Dy Magnitude difference (star1-star2) in y mag table.tex LaTeX version of table Patricia Bauer CDS 1994 Sep 01 J_A+AS_108_595.xml A Ca II and Mg II luminosity/emission-width data base J/A+AS/108/611 J/A+AS/108/611 CaII & MgII data base A Ca II and Mg II luminosity/emission-width data base E Lastennet R Freire Ferrero Astron. Astrophys. Suppl. Ser. 108 611 1994 1994A&AS..108..611L Combined data Stars, emission Stars, peculiar stars: catalogs stars: activity stars: chromospeheres The so-called Wilson-Bappu relationship (hereinafter W-B) is an empirical linear relation established in 1957. Formally simple, this relation links two observable parameters of a star: the CaII K line core emission width with the absolute magnitude of the star having chromospheric activity. Other Luminosity/Emission-width relationships were established on the basis of other chromospheric lines like MgII (2795.5A and 2802.7A) and Ly{alpha} (1215.9A). All these resonance lines are used as a diagnostic of physical properties of stellar chromospheres. We have reanalysed all the available data connected with the CaII K and the MgII k line widths in the literature from 1957 until today to be able to prepare a database containing all the essential information needed to study and to understand empirical stellar activity relationships.
Ca II K lines Ca II K lines: Kuhi data (Kuhi L.V., 1965, 1965PASP...77..253K) Mg II k line No Running number --- HD star's identification given by its HD number (except for some particular case like the `Sun', identified by its name) --- Sp Spectral type --- Cl Class of luminosity --- Mv Absolute magnitude, as provided in the papers we considered mag log(W) Decimal logarithm of the line width (emission line core; data provided only by the papers studied) number=1 In addition to the compilation of the original data, `summary' lines have been added for each star entered in the database. When the original emission-width's data were not corrected for the instrumental correction, we take into account this correction to calculate the FWHM (Ref 990) or the BASE (Ref 991) values. [km/s] Ref References number=2 Authors and relevant references entered by reference number (see table5 and table6 for the correspondence between the Ref number and the bibliographic sources). --- Vmag Visual magnitude mag B-V B-V colour mag U-B U-B colour mag vsini Rotational velocity km/s rem Remark V : variable star SB : spectroscopic binary e : emission star p : peculiar star CO : compagnon --- plx91 Weigthed average absolute parallax arcsec e_plx91 rms uncertainty on plx91 arcsec N Number of parallax observations included in weigthed average parallax --- q_plx91 Quality of the interagreement of different parallaxes observations (G = good, F = fair, P = poor) --- n_Binar Binarity of the collected stars when no number in the Aitken's catalog number=3 W : star listed in the Washington visual double Star Catalog A : Astrometric binary B : Spectroscopic binary E : Eclipsing binary O : Occultationary binary S : Speckle interferometric binary --- Binar Binarity of the collected stars. Nunber in the Aitken's catalog (ADS Catalog) --- V91 Visual magnitude mag Mabs91 Absolute magnitude computed from the columns Plx91 and V91 mag e_Mabs91 rms uncertainty on Mabs91. This column is computed from the columns Plx91 and e_Plx91 mag rel-e_Plx91 Relative error on the parallaxes given by the columns Plx91 and e_Plx91 arcsec Bibliographical sources for the Ca II k line Nref Reference number --- Type Type of measures --- Ref References --- N Number of distinct data --- ICorr Instrument correction --- Bibliographical sources for the Mg II K line Nref Reference number --- Type Type of measures --- Ref References --- Com Comments --- N Number of distinct data --- n_ICorr n = no correction --- ICorr Instrument correction 0.1nm tables.tex LaTeX version of tables Patricia Bauer CDS 1994 Jul 12 J_A+AS_108_611.xml Warm IRAS source from the point source catalog. IV. Extended optical line emission J/A+AS/108/61 J/A+AS/108/61 Warm IRAS source. IV. Warm IRAS source from the point source catalog. IV. Extended optical line emission G C Fehmers M H K De Grijp G K Miley W C Keel Astron. Astrophys. Suppl. Ser. 108 61 1994 1994A&AS..108...61F galaxies: active galaxies: ISM galaxies: Seyfert infrared: galaxies We present a list of objects observed to have extended line emission in our spectroscopic survey of infrared-warm AGN. Slit spectroscopic data were obtained for 225 galaxies identified with objects in our compendium of warm sources from the IRAS Point Source Catalog. Of these, 44 have spatially-resolved emission-line regions along the (arbitrarily placed) slit direction. Measured (projected) linear sizes of the ionized gas regions extend to >10kpc. In the case of the IRAS Seyfert galaxies the spatially extended line emission appears to have a lower ionization state than the nuclear emission. This contrasts with the warm IRAS starbust galaxies for which there is no significant difference between the ionization states of the nuclear and extended emission. For the starburst galaxies, there is a relation between the extent of star formation as seen at H{alpha} and the far-IR colors, with more compact bursts having "warmer" colors.
Galaxies with spatially unresolved line-emission No Running number as introduced in the catalogue of paper I. If the number is absent, the source does not appear in the catalogue (see paper) --- IRAS IRAS name --- PA1 First slit position angle deg PA2 Second slit position angle deg Galaxies with spatially extended or possibly extended line-emission No Running number, see table1 --- IRAS IRAS Name --- Name Alternative Name --- z Redshift --- AGN AGN spectral type --- o_IRAS Observing night number, see Paper II --- PA Slit position angle deg l_Asize limit flag on angular size --- Asize Angular size of line-emission arcsec l_Lsize limit flag on linear projected size --- Lsize Linear projected size, H=75 km/s/Mpc kpc Notes Notes number=1 1. Possibly extended. Stated size is uncertain. 2. IRAS 0032-617SW. This galaxy has a long tidal arm. The line profile along the slit has two peaks of emission, but the continuum profile has a single maximum. The line-emitting regions are about 4" apart and H II-type 3. IRAS 0033-819. A ring-shaped galaxy with two brightness enhancements, 11" apart, both strong line emitters. 4. IRAS 0141+020 (Markarian 573). The Seyfert-like emission extends out to 3.4" on either side of the nucleus, including relatively strong [O I]. This emission has been examined by Afanasiev & Sil'chenko (1991) and by Tsvetanov & Walsh (1992) from kinematic and ionization standpoints. 5. IRAS 0146-615. This galaxy has a long tidal arm. Along the slit, two peaks of emission are seen, both in line and continuum. The peaks are 8" apart and both are H II-type. 6. IRAS 0225-103 (Markarian 1039). This galaxy hosts two H II-type nuclei, 24" apart. 7. IRAS 0229-368 (IC 1816). The Seyfert-like spectrum extends as far as 3.4" east of the nucleus, including relatively strong [O I]. The nuclear [O III] lines are spectrally resolved, FWHM=900km/s, whereas the extended line-emission is narrower, FWHM<500km/s. 8. IRAS 0240-002 (NGC 1068). The nuclear emission lines have a FWHM of about 1200km/s, whereas the extranuclear emission is unresolved spectrally, FWHM<200km/s. 9. IRAS 0302-729. The nuclear emission lines are spectrally resolved, with FWHM=1300km/s, the extended emission lines are unresolved, FWHM<500km/s. 10. IRAS 0310-515. This galaxy has a long tidal arm. The brightness profile along the slit shows two peaks of emission, 7.4" apart. Both have Seyfert spectra. 11. IRAS 1703+606. An interacting pair, with a Seyfert and a starburst galaxy 6.5" apart, at almost the same redshift. 12. IRAS 1855+716. An interacting pair, two starburst galaxies 6.7" apart, almost same redshift. The line-emission (especially [O II]3727) forms a bridge between them. 13. IRAS 1908-539. This galaxy has a highly irregular morphology. The emission line- and continuum-profiles along the slit show double structure, two peaks separated by 20". One has a Seyfert spectrum and the other is H II-type. 14. IRAS 2048-572 (PKS 2048-57). This object has a Seyfert-like spectrum extending by at least 4" on either side of the nucleus, including relatively strong [O I]. There is a large velocity gradient, the emission lines 3" east and west of the nucleus being shifted by 230km/s red- and bluewards respectively, relative to the nucleus. 15. IRAS 2117-492. An interacting pair of starburst galaxies 41" apart, at almost the same redshift. The line emission in the eastern galaxy is extended by at least 24". --- table1.tex LaTeX version of table1 table2a.tex LaTeX version of table2 (left part) table2b.tex LaTeX version of table2 (right part) Patricia Bauer CDS 1994 Sep 23 J_A+AS_108_61.xml The distribution of dust in Sb's and Sc's - K-band infrared imaging of a diameter limited sample of 37 galaxies J/A+AS/108/621 J/A+AS/108/621 Dust in Sb and Sc K-band The distribution of dust in Sb's and Sc's - K-band infrared imaging of a diameter limited sample of 37 galaxies R F Peletier E A Valentijn A F M Moorwood W Freudling Astron. Astrophys. Suppl. Ser. 108 621 1994 1994A&AS..108..621P galaxies: ISM galaxies: photometry galaxies: spiral galaxies: structure infrared: galaxies We present deep infrared K-band surface photometry for a diameter-limited sample of normal Sb and Sc galaxies. In addition, surface brightness, optical and optical-infrared colors and isophote-shapes have been obtained from the ESO-LV B and R photographic images of these galaxies. For each galaxy we present global photometric parameters, as well as individual radial surface brightness and color profiles. Our analysis includes the fitting of ellipses in the three bands, bulge-disk decompositions, and the derivation of growth curves in elliptical apertures. The main conclusion of the paper is that these galaxies exhibit very large color gradients - B and K scale length ratios vary between 1.2 and 2.0 and increase with axis ratio. The large magnitude of these gradients suggest that they are not due to stellar population differences, but are primarily due to extinction by dust in the B-band. We also find that the range of central surface brightnesses in the K-band is considerably larger than in B, showing that the stellar properties are better studied in K. A more detailed evaluation of the results, specifically with regard to the spatial distribution of both the dust and the stars in Sb and Sc galaxies, will be presented in an accompanying paper (Peletier et al. 1994, Paper II).
Surface photometry and colors Name Source name --- Rad Radius (sqr(ab)) arcsec Mu(K) Surface brightness in K band mag/arcmin2 B-R B-R colour mag e_B-R rms uncertainty on B-R mag B-K B-K colour mag e_B-K rms uncertainty on B-K mag Epsilon Ellipticity (1-b/a) --- Phi Position angle in K band deg Patricia Bauer CDS 1994 Aug 29 J_A+AS_108_621.xml The low galactic latitude metal-rich globular cluster NGC 6440 J/A+AS/108/653 J/A+AS/108/653 NGC 6440 The low galactic latitude metal-rich globular cluster NGC 6440 S Ortolani B Barbuy E Bica Astron. Astrophys. Suppl. Ser. 108 653 1994 1994A&AS..108..653O globular clusters: general globular clusters: individual (NGC 6440) Hertzsprung-Russell (HR diagram) NGC 6440 is another case of bulge high metallicity globular cluster with particular colour magnitude diagram properties, like those of NGC 6553, NGC 6528 and Terzan 1. We present V and I observations of NGC 6440, and find a reddening of E(B-V)=~1.00+/-0.1, and a distance of d_{sun}_=~8.47kpc. The colour magnitude diagram morphology shows characteristics very similar to those of NGC 6553 and NGC 6528, in particular the horizontal branch clump almost superimposed on the giant branch, and a curved upper giant branch, showing that NGC 6440 also has a metallicity close to solar.
V, I photometry of NGC 6440 No Sequential number --- X X pixel coordinate as in Fig. 1 pix Y Y pixel coordinate as in Fig. 1 pix Vmag V magnitude mag V-I V-I colour mag Patricia Bauer CDS 1994 Aug 29 J_A+AS_108_653.xml Low resolution IUE spectra of Wolf-Rayet stars. J/A+AS/108/669 J/A+AS/108/669 IUE spectra of WR stars Low resolution IUE spectra of Wolf-Rayet stars. A Niedzielski K Rochowicz Astron. Astrophys. Suppl. Ser. 108 669 1994 1994A&AS..108..669N atlases stars: classification stars: Wolf-Rayet We present uniformly reduced and measured equivalent widths, FWHM and observed line fluxes for 94 "single" WR stars (34 galactic WN, 22 galactic WC, 31 LMC WN and 7 LMC WC) based on the archive IUE spectra of WR stars gathered from different observational runs and from different epochs. The spectra are used for spectral classification in the ultraviolet region and for searching correlations among the strength and widths of emission lines of different ions. Some correlations with optical and near IR lines observed by other authors are given as well. The set of spectra we use is almost complete to 12 magnitude and representative according to spectral subtype of WR stars.
Low resolution IUE spectra Gal Star membership, galaxy or LMC --- Type Star type, WN or WC --- Name Star name --- Line Identification observed wavelength 0.1nm LogW Equivalent width 0.1nm FWHM Full width at half maximum 0.1nm Flux Observed (reddened) flux in a line 10mW/m2/nm tabwcg.tex LaTeX version of table6 for galactic WC stars tabwcl.tex LaTeX version of table6 for LMC WC stars tabwng.tex LaTeX version of table6 for galactic WN stars tabwnl.tex LaTeX version of table6 for LMC WC stars Patricia Bauer CDS 1994 Sep 19 J_A+AS_108_669.xml Samples of ultra-steep spectrum radio sources J/A+AS/108/79 J/A+AS/108/79 Ultra-steep spectrum radiosources Samples of ultra-steep spectrum radio sources H J A Roettgering M Lacy G K Miley K C Chambers R Saunders Astron. Astrophys. Suppl. Ser. 108 79 1994 1994A&AS..108...79R Radio sources surveys galaxies: active radio continuum: galaxies Radio sources with ultra-steep spectra (USS; spectral index <~ -1.0) have been found to be excellent tracers of galaxies at redshifts z>~2. The samples are selected from the set of catalogues referenced below, in a range of frequencies from 38 to 408MHz; they are are fainter by a factor of three than the previously well-studied samples of USS sources from 4C. Snapshot observations of sources from these samples have been made with the VLA at 1.5arcsec resolution and are presented in the printed paper. The list of the sources (Appendix A of the paper) includes positions, flux densities and radio structures for a total number of 605 sources derived from these observations.
Source list Samples Name of the samples to which the source belongs number=1 the 9 samples are defined in Table 4 of the paper; the names are related to the lowest frequency (MHz): 408A, 408B, 365A, 365B, 178, 151I, 38A, 38B, 38C --- Name Source name in IAU B1950.0 format --- m_Name Component designator number=2 the component indicator may be: - a number indicates that the component belongs to the main central radio source. A 'c' after a number indicates that this component is probably the core component. - a letter indicates that the object is bright (presumably) serendipitous source visible in the VLA map in a 4'x4' region surrounding the source. --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec RAh1950 Right ascension B1950 h RAm1950 Right ascension B1950 min RAs1950 Right ascension B1950 s DE-1950 Declination sign --- DEd1950 Declination B1950 deg DEm1950 Declination B1950 arcmin DEs1950 Declination B1950 arcsec Speak Peak brightness mJy Sint Integrated flux density mJy R Ratio of the integrated VLA flux density to the flux density obtained from the NRAO Green Bank 1400 MHz --- alpha(l) Low frequency spectral index --- e_alpha(l) Rms uncertainty on alpha(l) --- alpha(h) High frequency spectral index --- e_alpha(h) Rms uncertainty on alpha(h) --- Cat Radio catalogues that have been used in the spectral index calculations number=3 the catalogues are a: 8C(38 MHz) <1990MNRAS.244..233R> b: PKS(80 MHz) <VIII/15> c: 6C2(151 MHz) <VIII/21> d: PKS(178 MHz) <VIII/15> e: TXS(365 MHz) The Texas Survey (see Douglas et al, 1980, Univ. Texas Publ. in Astronomy 17, 1) f: TXS:BWE(365 MHz) g: PKS(408 MHz) <VIII/15> h: MRC(408 Mhz) <VIII/16> i: NRAO(1400 MHz) <VIII/6> j: WB(1400 MHz) <VIII/17> k: PKS(1410 MHz) <VIII/15> l: VLA(1465 MHz) m: PKS(2700 MHz) <VIII/15> n: NRAO(4850 MHz) <VIII/6> o: 87GB(4580 MHz) <VIII/14> p: BWE(4589 MHz) <VIII/13> q: WB(4580 MHz) <VIII/17> r: PKS(5000 MHz) <VIII/15> --- n_Cat Notes on catalogues number=4 Various flags indicating catalogue problems and/or confusion: Flags a to h have been directly copied from three catalogues at 1400 and 4850 MHz (WB, BWE and 87GB). Flags r to x indicate inconsistencies and how various upper limits have been treated. *: The spectral index/indices is/are unreliable, since there are warnings in one of the three 1400/4580 MHz catalogues (a to h) and/or there is a bright confusing source in the VLA field (z) a: In WB a 1400 MHz source is reported to match more than one 1400 MHz or 365 MHz source so that confusion is likely b: In WB a 1400 MHz source is reported to be extended at 1400 MHz c: In WB a 1400 MHz source is reported to be extended at 4850 MHz d: In BWE a 4850 MHz source is reported to be extended at 4850 MHz Note that the flags c and d are not always simultaneously present e: In the BWE the separation between the NRAO 4850 MHz and the Texas 365 MHz positions is reported to be greater than 100 arcsecs f: In 87GB a source is reported to be extended or a blend of two or more point sources (Flag E in the original catalogue) g: In 87GB a source has a warning that it is a weak source with a large zero offset, a narrow minor axis, or possibly confused; less reliable than most (Flag W in the original catalogue) h: In 87GB a source is reported to be confused (Flag C in the original catalogue) q: Difference of 4850 MHz flux densities of 87GB and our fitting routines are greater than 10 mJy r: Difference in the 365 MHz flux densities from the version of the Texas catalogue that we used and the version that WB used u: Since no Texas flux density is present in WB catalogue, we used the flux density from our version of the Texas Catalogue v: No 1400 MHz flux densities in WB w: Since no 4850 MHz flux densities is present in WB, we used the 87GB 4850 MHz flux density x: No WB and 87GB 4850 MHz flux densities. Our determination for the 4850 MHz NRAO flux densities is used if this flux density >15mJy z: A bright serendipitous source in the VLA field Notes on individual sources: 0141+356 A serendipitous double radio galaxy in the field is present about 1.5 minutes from components `1' and `2'. 0309-047 Component `A' is probably serendipitous. 0707+810 This is resolved into two separate sources. The northern source has an asymmetric FRII structure; the southern a bright central component and low surface brightness lobes just detectable on the low-resolution VLA map. CLFST observations show that both sources have similar fluxes at 151-MHz (~100 mJy for the northern source and ~150 mJy for the southern), but the southern source has a steeper spectral index; hence this object should dominate the flux at the selection frequency of 38-MHz. 0906+691 The VLA map shows three diffuse components; a CLFST map shows two distinct sources, the southern of which is resolved into two components and may therefore either be a single large source or two smaller ones. 1127+831 A Ryle Telescope map at 5GHz [calibrated and analysed as detailed in Lacy et al. (1993)] only detects component 1, but shows it to have a very steep radio spectrum (alpha^{1490}^_{5000}_=-1.1), suggesting that it is some form of hotspot. 1227+609 It is not clear whether the three components are related. 1323+080 It is not clear if component `2' is real. 1345-309 Diffuse radio source. Coordinates are derived from the moments of the source brightness. 1350+635 This 80 arcsec source has a faint central component and diffuse lobes which barely show up on the VLA map. CLFST observations confirm the presence of the lobes. 1436+157 The double radio galaxy with components 'A' and 'B' is probably not related to the double radio galaxy with components '1' and '2'. 1611+452 It is not clear whether the three components belong to one source. 1652+027 Two components separated by 233", so may not be a single source. 1659+440 Component A probably is probably a separate serendipitous source. 1718+630 Component '1' serendipitous or related to double radio source? 1942+631 Component A related to central radio source ? 2207+038 It is not clear whether the two components belong to one source. 2324+071 Diffuse double lobed radio source. Position of lobes measure from the tapered maps. 2335-125 It is not clear whether the two components belong to one source. --- Mul D = double, P = point source, T = triple DF = diffuse, M = complex --- l_Size Limit flag on Size --- Size Angular size measured from VLA maps arcsec PA Position angle measured from VLA maps deg source.tex LaTeX version of source Patricia Bauer CDS 1994, rev. Francois Ochsenbein 19-Aug-1996 Jul 01 J_A+AS_108_79.xml Fundamental parameters of Cepheids: I. Photometric data in the Geneva system J/A+AS/108/9 J/A+AS/108/9 Cepheids fundamental parameters I. Fundamental parameters of Cepheids: I. Photometric data in the Geneva system D Bersier G Burki M Burnet Astron. Astrophys. Suppl. Ser. 108 9 1994 1994A&AS..108....9B Cepheids stars: oscillations Photometric data in the Geneva system for 26 Cepheid stars are given, representing 869 individual measurements. After a short explanation on the analysis, the choice of the period and the quality of the fit of the light curve are discussed. The data and the fitted light- and colour curves are given, as well as the Fourier coefficients of the best fit for each star.
Geneva photometry for 26 Cepheids Name Star name --- HD HD number or BD number or coordinates 1900 --- JD Date of measurement d WV Weight of the measurement of V magnitude --- Vmag V magnitude mag WC Weight of the measurement of the colours --- [U-B] U-B colour mag [V-B] V-B colour mag [B1-B] B1-B colour mag [B2-B] B2-B colour mag [V1-B] V1-B colour mag [G-B] G-B colour mag Patricia Bauer CDS 1994 May 26 J_A+AS_108_9.xml Analytic fits for partial photoionization cross sections J/A+AS/109/125 J/A+AS/109/125 Photoionisation cross section Analytic fits for partial photoionization cross sections D A Verner D G Yakovlev Astron. Astrophys. Suppl. Ser. 109 125 1995 1995A&AS..109..125V atomic data atomic processes We present a uniform, compact and complete set of fit parameters to the cross sections for all subshells of atoms and ions of the elements under study. The partial photoionisation cross sections {sigma}_nl_(E) will be described by the fitting formula (equation 1): {sigma}_nl_(E)={sigma}_0_xF(E/E_0_) (in Mb), F(y)=[(y-1)^2^+(y_w_)^2^]y^-Q^[1+sqr(y/y_a_)]^-P^, where n is the principal quantum number of the shell, l=0, 1, 2 (or s, p, d) is the subshell orbital quantum number, E is the photon energy in eV, y=E/E_0_; {sigma}_0_, y_w_, y_a_ and P are the fit parameters, and Q=5.5+l-0.5P.
Fit parameters for partial photoionization cross sections Z Atomic number --- N Number of electrons --- n Principal quantum number of the shell --- l Orbital quantum number of the subshell --- E(th) Subshell ionization threshold energy eV E(0) Fit parameter of equation 1 eV sigma(0) Fit parameter of equation 1 Mbarn y(a) Fit parameter of equation 1 --- P Fit parameter of equation 1 --- y(w) Fit parameter of equation 1 --- Patricia Bauer CDS 1994 Sep 02 J_A+AS_109_125.xml The ROSAT AGN content of the 87GB 5GHz survey: bulk properties of previously optically identified sources J/A+AS/109/147 J/A+AS/109/147 ROSAT AGN content The ROSAT AGN content of the 87GB 5GHz survey: bulk properties of previously optically identified sources W Brinkmann J Siebert W Reich E Fuerst P Reich W Voges J Truemper R Wielebinski Astron. Astrophys. Suppl. Ser. 109 147 1995 1995A&AS..109..147B III/175 : Optical spectroscopy of radio sources (Stickel+, 1989-94) VIII/14 : 87GB Catalog of radio sources (Gregory et al., 1991) Active gal. nuclei Radio sources X-ray sources galaxies: active quasars: general radio sources: general X-rays: general The cross-correlation of the source list from the ROSAT All-Sky Survey with the 5 GHz Green Bank survey yields a list of 2127 objects. About two thirds of them are optically unidentified. The majority of the objects with known optical counterparts are quasars and radio galaxies, most of them detected in X-rays for the first time. In this paper we present a list of the previously optically identified objects with their main characteristics and discuss their general (bulk) properties. We find strong correlations between luminosities in the radio, optical, and X-ray bands which differ for quasars and radio galaxies.
ROSAT
Catalog of sources from RASS-Condon correlation ROSAT ROSAT name of source --- Class Object class (reference r_Vmag) --- Type Optical type number=4 the optical type is a defined in NED: E = Elliptical ; S = Spiral ; I = Irregular ; SY1,2 = Seyfert type 1,2 HP = Highly polarized in the optical ; 0,1,2 = richness class for Clusters of Galaxies GPA = Galaxy pair ; GTR = Galaxy triple --- Name Other name of source --- r_Vmag Reference for the optical identification and data if not from NED number=1 References for optical identification, Vmag and z are: 1: Stickel and Kuehr (1994A&AS..103..349S); in catalog <III/175> 2: Stickel and Kuehr (1993A&AS..100..395S); in catalog <III/175> 3: Stickel and Kuehr (1993A&AS..101..521S); in catalog <III/175> 4: Stickel and Kuehr (1994A&AS..105...67S) 5: Kock A., private communication 6: Bade N., et al. (1994A&A...286..381B) 7: Fleming T.A., et al., 1994, ApJ (in press?) --- Vmag Optical magnitude mag z Redshift --- F5GHz 5GHz radio flux density Jy e_F5GHz rms uncertainty on F5GHz Jy q_F5GHz Error class from Bonn catalog number=3 For the Bonn catalog, the error class on F5GHz is 1: <= 9%; 2: 9-14% ; 3: 14-23% ; 4: >= 23% --- r_F5GHz Reference for radio flux number=2 B = Bonn catalog: error class is available (see q_F5GHz) C = Gregory & Condon 87GB <VIII/14> catalog. --- FX X-ray flux in (0.1-2.4)keV energy band 10-14W/m2 e_FX rms uncertainty on X-ray flux 10-14W/m2 Dist Distance between radio and X-ray position arcsec Patricia Bauer CDS 1994; revised F. Ochsenbein 13-May-1996 Sep 02 J_A+AS_109_147.xml A catalog of blue horizontal branch stars in the outer galactic halo J/A+AS/109/171 J/A+AS/109/171 Blue horizontal branch stars catalog A catalog of blue horizontal branch stars in the outer galactic halo C Flynn J Sommer-Larsen P R Christensen M R S Hawkins Astron. Astrophys. Suppl. Ser. 109 171 1995 1995A&AS..109..171F Galaxy: halo Galaxy: kinematics and dynamics stars: horizontal-branch We present a sample of faint blue stars at medium to high galactic latitude, and classify the stars as blue horizontal branch (BHB) or probable non-BHB stars on the basis of medium dispersion spectra and broadband photoelectric BV photometry. The classification scheme (Flynn et al. 1993) is as accurate as Stroemgren photometry. Using this method we have identified a sample of 100 BHB objects in the galactic halo to faint magnitudes (13.5 < V < 19.5), the selection criteria ensuring that the sample is the cleanest to date. We analyse the kinematics of the BHB stars in a subsequent paper.
F117 field (l = 270deg, b = -45deg) 22h field (l = 38deg, b = -51deg) SA287 field (l = 0deg, b = -47deg) South Galactic Pole field ID Star name --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Vmag V magnitude mag B-V B-V colour mag o_B-V Number of observations in B and V --- n_o_B-V A '*' indicates BV data derived from transformed Stroemgren photometry --- DM Hydrogen line width index --- Class Classification BHB = blue horizontal branch, ? = unknown --- RV Heliocentric radial velocity km/s Dhel Estimated heliocentric distance kpc Dgal Estimate galactocentric distance kpc Note Notes on the observations number=1 Numbers indicate the sources or dates of observations of the photometry, while the letters indicate the sources or dates of observation of the spectroscopy. 1: photoelectric photometry from Flynn and Sommer-Larsen (1998) 2: CCD photometry from Flynn, Sommer-Larsen and Christensen (1994) 3: new CCD data from the ESO 1.5m (Sept. 1990, Sept. 1991 and Aug. 1992) A: data from Sommer-Larsen and Christensen (1986) B: data from Sommer-Larsen and Christensen (1987) C: data from Sommer-Larsen, Christensen and Carter (1989) D: ESO 2.2m, Nov. 1987 E: MSSSO 2.3m, Aug. 1998 F: ESO 2.2m, Sep. 1998 G: ESO 2.2m, Aug. 1989 H: ESO 2.2m, Nov. 1990 I: ESO 3.5m, New Technology Telescope, Sep. 1991 and Aug. 1992 --- Patricia Bauer CDS 1994 Sep 21 J_A+AS_109_171.xml Representation of planetary ephemerides by frequency analysis. Application to the five outer planets. J/A+AS/109/181 J/A+AS/109/181 Planetary ephemerides Representation of planetary ephemerides by frequency analysis. Application to the five outer planets. J Chapront Astron. Astrophys. Suppl. Ser. 109 181 1995 1995A&AS..109..181C ephemerides methods: numerical planets and satellites: general Heliocentric equatorial rectangular coordinates of the five outer planets (X, Y and Z). The source is based on DE200 (tables 4 to 7) or a reconstruction of DE200 by numerical integration (tables 9 to 13). The reference frame is the mean equator and equinox J2000 of DE200. The general formulation of the series X is: X = SUM[i=1,Records] T**n_i*(CX_i*cos(Nu_k*t)+SX_i*sin(Nu_k*t)) The formulation is identical for Y and Z. T is the time (TDB) in Julian centuries from J2000: T = (JulianDate - 2451545.0)/36525 t is the time (TDB) in Julian years from J2000: t = (JulianDate - 2451545.0)/365.25 Nu is the frequency. Frequencies are identical for all terms of rank k: Nu_k = Nu_i when n_i = 0 For purely secular terms k = 0 and Nu_0 = 0
*Jupiter *Saturn *Uranus *Neptune *Jupiter *Saturn *Uranus *Neptune *Pluto k Rank of the frequency --- n Power of time number=1 If n=0 the term is purely periodic (Fourier) or constant. If n=1,2 or 3 the term is mixed (Poisson) or secular, of degree 1, 2 or 3 with respect to time --- CX Variable X - Cosine term number=2 Units are 1e-10 AU if n=0, 1e-10 AU/Cy if n=1, 1e-10 AU/Cy2 if n=2, 1e-10 AU/Cy3 if n=3 --- SX Variable X - Sine term number=2 Units are 1e-10 AU if n=0, 1e-10 AU/Cy if n=1, 1e-10 AU/Cy2 if n=2, 1e-10 AU/Cy3 if n=3 --- CY Variable Y - Cosine term number=2 Units are 1e-10 AU if n=0, 1e-10 AU/Cy if n=1, 1e-10 AU/Cy2 if n=2, 1e-10 AU/Cy3 if n=3 --- SY Variable Y - Sine term number=2 Units are 1e-10 AU if n=0, 1e-10 AU/Cy if n=1, 1e-10 AU/Cy2 if n=2, 1e-10 AU/Cy3 if n=3 --- CZ Variable Z - Cosine term number=2 Units are 1e-10 AU if n=0, 1e-10 AU/Cy if n=1, 1e-10 AU/Cy2 if n=2, 1e-10 AU/Cy3 if n=3 --- SZ Variable Z - Sine term number=2 Units are 1e-10 AU if n=0, 1e-10 AU/Cy if n=1, 1e-10 AU/Cy2 if n=2, 1e-10 AU/Cy3 if n=3 --- Nu Frequency rad/yr Patricia Bauer CDS 1994 Oct 03 J_A+AS_109_181.xml Atomic data from the IRON project. VIII. Electron excitation of the 3d^4^ ^5^D_J_ ground state fine-structure transitions in Ti-like ions V II, Cr III, Mn IV, Fe V, Co VI and Ni VII J/A+AS/109/193 J/A+AS/109/193 IRON project VIII. Ti-like ions Atomic data from the IRON project. VIII. Electron excitation of the 3d^4^ ^5^D_J_ ground state fine-structure transitions in Ti-like ions V II, Cr III, Mn IV, Fe V, Co VI and Ni VII K A Berrington Astron. Astrophys. Suppl. Ser. 109 193 1995 1995A&AS..109..193B J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions =1993A&A...279..298H : IRON Project I. Goal and methods =1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions =1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion =1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths =1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure =1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation =1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation =1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition =1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI =1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data Electron excitation collision strengths for the 3d^4^ ^5^D(J-J') ground term fine-structure transitions in titanium-like ions V II, Cr III, Mn IV, Fe V, Co VI and Ni VII are calculated using R-matrix techniques. The model target ion includes all 3d^4^ terms, and the low-energy collision strengths are dominated by autoionizing resonances. The collision strength is averaged over a Maxwellian velocity distribution to obtain effective collision strengths as a function of electron temperature. To our knowledge, these are the first published data for these processes.
Fine-structure energy levels of the 3d^4^ ^5^D_J_ ground state Ion Ion --- Ref Calculation mode of theoretical energies number=1 0: Current Breit-Pauli calculation 1: Moore C.E., 1971, NSRDS-NBS 35 vols. I & II 2: Sugar J. and Corliss C., 1977, J. Phys. Chem. Ref. Data, 6, 343 3: Corliss C. and Sugar J., 1977, J. Phys. Chem. Ref. Data 4, 1293 4: Reader J. and Sugar J., 1975, J. Phys. Chem. Ref. Data, 4, 400 5: Corliss C. and Sugar J., 1981, J. Phys. Chem. Ref. Data 10., 258 --- E0 Theoretical energy at J=0 Ry E1 Theoretical energy at J=1 Ry E2 Theoretical energy at J=2 Ry E3 Theoretical energy at J=3 Ry E4 Theoretical energy at J=4 Ry Effective collision strengths for 3d^4^ ^5^D_J-J'_ fine-structure transitions Ion Ion --- Level Initial and final J and J' levels --- gamma1 Effective collision strength for log(T)=3.0K --- gamma2 Effective collision strength for log(T)=3.2K --- gamma3 Effective collision strength for log(T)=3.4K --- gamma4 Effective collision strength for log(T)=3.6K --- gamma5 Effective collision strength for log(T)=3.8K --- gamma6 Effective collision strength for log(T)=4.0K --- gamma7 Effective collision strength for log(T)=4.2K --- gamma8 Effective collision strength for log(T)=4.4K --- gamma9 Effective collision strength for log(T)=4.6K --- gamma10 Effective collision strength for log(T)=4.8K --- gamma11 Effective collision strength for log(T)=5.0K --- gamma12 Effective collision strength for log(T)=5.2K --- gamma13 Effective collision strength for log(T)=5.4K --- gamma14 Effective collision strength for log(T)=5.6K --- gamma15 Effective collision strength for log(T)=5.8K --- gamma16 Effective collision strength for log(T)=6.0K --- gamma17 Effective collision strength for log(T)=6.2K --- gamma18 Effective collision strength for log(T)=6.4K --- Patricia Bauer CDS 1994 Sep 22 J_A+AS_109_193.xml CCD photometry of the globular clusters NGC 6496, NGC 6624, and NGC 6637 J/A+AS/109/1 J/A+AS/109/1 CCD photometry of globular clusters CCD photometry of the globular clusters NGC 6496, NGC 6624, and NGC 6637 T Richtler Astron. Astrophys. Suppl. Ser. 109 1 1995 1995A&AS..109....1R globular clusters: general globular clusters: individual (NGC 6496, NGC 6624, NGC 6637) Presents the data part of work concerning the age, metallicity, and distance of three globular clusters, which are believed to belong to the disk system of galactic globular clusters, NGC 6496, NGC 6624, and NGC 6637 (M69). Information is given on: the observations, the reduction, the photometric calibration. A new photoelectric sequence around NGC 6496 is presented as well. The present data are compared with previous work. Finding charts as well as recipes for cross identification are given. Lists containing the brighter stars in the cluster regions are added.
NGC 6496 NGC 6624 NGC 6637 Seq Sequence --- X X position pix Y Y position pix Vmag V magnitude mag e_Vmag rms uncertainty on V mag B-V B-V colour mag e_B-V rms uncertainty on B-V mag Patricia Bauer CDS 1994 Jul 01 J_A+AS_109_1.xml A catalogue of variable stars in the lower instability strip J/A+AS/109/201 J/A+AS/109/201 Catal. of variable stars in instability strip A catalogue of variable stars in the lower instability strip J R Garcia J R Cebral E R Scoccimarro P Wahnon R Arena V Bazterra L Pellizza A Risi M L Rodriguez M Zimmermann Astron. Astrophys. Suppl. Ser. 109 201 1995 1995A&AS..109..201G catalogs delta Scuti stars: variables: other Identifications, positions, photometry, spectra, some pulsational features, other astrophysical parameters and literature for 302 pulsating variable stars in the lower instability strip, near the ZAMS, are given. About 185 stars have near homogeneous photometric information in the Stroemgren's uvby-{beta} photometric system. This catalogue/database covers information published until November 1993.
*Identification, type of variability and astrometrical data for 302 Delta Sct stars Name Star's name and constellation --- HD HD Number --- HR HR Number --- Var Type of variability number=1 According to the General Calalogue of Variable Stars, 4th edition --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin GLON Galactic longitude deg GLAT Galactic latitude deg PreRA Precession in right ascension (1950.0) s PreDE Precession in declination (1950.0) arcmin *Astrophysical data (UBV and ubvy-beta photometry and rotational velocity) for most of the stars Name Star's name and constellation --- HD HD Number --- HR HR Number --- Period Period d Date Epoch (Julian Date) d Magmax Magnitude in maximum light mag Magmin Magnitude in minimum light mag MagType Type of magnitude used in the last two data number=1 Type of magnitude may be B, V (from UBV system) or P (photographic). --- A Amplitude mag Mv Absolute magnitude, Mv mag b-y b-y colour mag (b-y)0 (b-y)0 colour mag m1 m1 colour index mag m0 m0 colour index mag Dm1 Delta m1 mag D[m1] Delta [m1] mag Beta Beta magnitude mag E(b-y) E(b-y) mag c1 c1 colour index mag c0 c0 colour index mag Dc1 delta c1 mag D[c1] delta [c1] mag Vmag V magnitude mag B-V B-V colour mag U-B U-B colour mag Vrot Rotational velocity v.sin(i) km/s *Additional information. Spectral type, radial velocities, proper motion and parallax for most of the stars Name Star's name and constellation --- HD HD Number --- HR HR Number --- Sp Spectral Type and Luminosity Class number=1 The spectral type is in the MK system, when available. A "-" sign between two spectral types means that they are the limits of spectral type variation. A "+" sign between two spectral types means that the spectrum is complex, and two or more components were identified. --- RV Radial velocity km/s e_RV rms uncertainty on radial velocity km/s u_RV uncertainty flag on RV --- pmRA Proper motion in right ascension arcsec/yr e_pmRA rms uncertainty on pmRA arcsec/yr pmDE Proper motion in declination arcsec/yr e_pmDE rms uncertainty on pmDE arcsec/yr plx Parallax arcsec e_plx rms uncertainty on parallax arcsec Remarks Name Star name --- Rem Remarks --- References in literature Name Star name --- Ref References numbers --- References No References number --- Ref References --- Patricia Bauer CDS 1994 Nov 10 J_A+AS_109_201.xml Opacity sampling model photospheres for M dwarfs. II. The grid J/A+AS/109/263 J/A+AS/109/263 M dwarfs model photospheres. II. Opacity sampling model photospheres for M dwarfs. II. The grid J M Brett Astron. Astrophys. Suppl. Ser. 109 263 1995 1995A&AS..109..263B stars: atmospheres stars: fundamental parameters stars: late-type stars: low-mass, brown dwarfs We present a table of new "classical" model photospheres for M dwarfs computed with an extensive set of atomic and molecular opacities treated with the accurate and realistic opacity sampling technique. The models of this grid are described and analysed in a companion paper (Brett 1995, A&A, in press)
Model structure Teff Effective temperature K logg Surface gravity cm/s2 log(z) Metal abundance (given as a decimal logarithmic value relative to the solar abundance) Sun tau(R) Rosseland optical depth --- log(ChiR) Rosseland mean opacity cm2/g Tgas Gas temperature K log(Pg) Gas pressure 10Pa log(Pe) Electron pressure 10Pa log(Rho) Density g/cm3 log(Grad(ad)) Adiabatic temperature gradient K/cm F(conv) Fraction of the convective to total flux --- Patricia Bauer CDS 1994 Sep 16 J_A+AS_109_263.xml Radio to X-ray energy distribution of BL Lacertae objects J/A+AS/109/267 J/A+AS/109/267 Radio to X-Ray distribution of BL Lac Objects Radio to X-ray energy distribution of BL Lacertae objects P Giommi S G Ansari A Micol Astron. Astrophys. Suppl. Ser. 109 267 1995 1995A&AS..109..267G BL Lacertae objects: general radio continuum: galaxies X-rays: galaxies We present multifrequency spectra of a large number of radio and X-ray selected BL Lacertae objects constructed using non-simultaneous archival data. The data were obtained using the European Space Information System (ESIS) and are from several radio and optical catalogues, the IRAS Faint Source Catalogue, the Einstein and the EXOSAT databases. The sample includes 121 BL Lacs that have been extracted from the 1Jy and the S4 radio surveys (Stickel et al. 1991; Stickel & Kuehr 1994), the Einstein IPC Slew Survey, the Einstein Extended Medium Sensitivity Survey (EMSS), the EXOSAT High Galactic Latitude Survey, and from the compilations of Giommi et al. (1990), and Veron & Veron (1993). We find that the shape of the radio to infra-red spectrum of Radio Selected and X-ray Selected BL Lacs is very similar. The difference between these two classes of objects is instead evident in the optical/X-ray part of the spectrum. The classical radio discovered BL Lacs are characterized by an energy spectrum with a sharp cutoff in the IR/optical band while in most of the X-ray discovered objects the turnover is located near the UV/X-ray band or at higher frequencies. For a given X-ray flux this diversity can give rise to radio fluxes different by a factor of 100 or more. We argue that BL Lac objects may be a single population of sources characterized by a wide range of energy cutoffs. In this scenario BL Lacs discovered in radio surveys are representative of the entire population, while objects characterized by an energy break near the X-ray band, which are abundantly detected at X-ray frequencies, are intrinsically a small minority.
Radio selected BL Lacs 1Jy and S4 surveys X-ray selected BL Lacs from the Einstein IPC Slew Survey Serendipitous X-ray BL Lacs Einstein EMSS and EXOSAT HGLS Miscellaneous BL Lacs Name Source name --- Other Other names --- RAh Right ascension 2000.0 h RAm Right ascension 2000.0 min RAs Right ascension 2000.0 s DE- Declination sign --- DEd Declination 2000.0 deg DEm Declination 2000.0 arcmin DEs Declination 2000.0 arcsec Ref References number=1 1 Elvis at al. 1992 2 Gioia et al. 1990 3 Giommi et al., 1990 4 Giommi et al. 1991 5 Schachter et al. 1993 6 Stickel et al.1991 7 Stickel & Kuehr 1994 8 Stocke et al. 1991 9 Veron & Veron, 1993 --- Multifrequency data Name Source name --- nu Frequency Hz SX Flux in the X-ray band, where the measurements are often near the instruments sensitivity limit mW/m2 e_SX rms uncertainty on flux mW/m2 Ref References where the original flux (or count rate) can be found number=1 1 Becker, White & Edwards, 1991 2 Bolton Savage & Wright, 1979 3 Elvis et al. 1992 4 Dixon 1976 5 Giommi et al. 1990 6 Giommi et al. 1991 7 Moshir 1991 8 Stocke et al. 1991 9 Stickel & Kuer 1994 10 Veron & Veron 1993 11 White & Becker 1992 12 Einstein IPC database 13 EXOSAT database --- Patricia Bauer CDS 1995 Feb 24 UNKNOWN UNKNOWN * Table 5 was incomplete before Feb. 24, 1995. J_A+AS_109_267.xml Heterochromatic extinction. I. Dependence of interstellar extinction on stellar temperature, surface gravity, and metallicity. J/A+AS/109/293 J/A+AS/109/293 Heterochromatic extinction. I. Heterochromatic extinction. I. Dependence of interstellar extinction on stellar temperature, surface gravity, and metallicity. E K Grebel W J Roberts Astron. Astrophys. Suppl. Ser. 109 293 1995 1995A&AS..109..293G dust, extinction stars: fundamental parameters techniques: photometric Techniques used to remove atmospheric extinction cannot be used for interstellar extinction, because objects can be observed at only a single extinction, which varies from object to object. The interstellar extinction is thus unknowable without the use of prior information about the object. In this paper we show how to apply such knowledge in the case of normal stars. Using standard passbands, an accepted average optical interstellar extinction law, and Kurucz flux tables, we derive useful colour-dependent interstellar extinction relations for synthetic versions of two widely used sets of broad band photometric passbands, Johnson-Cousins UBVRI and Washington CMT_1_T_2_. For the Washington system, we define a new internal reddening system. For bands blueward of 500 nm in either photometric system the reddenings for main sequence stars and evolved stars are quite different, and even can be non-linear as a function of temperature colour. These corrections are important for the correct characterisation of the intrinsic reddening properties of interstellar dust, for fitting isochrones accurately, for determining stellar metallicities, for obtaining correct standard reddenings for reddened galactic clusters, and indeed for the determination of basic stellar parameters for single stars such as T_eff_ and M_bol_. To make the reddenings to different objects comparable, we standardise the reddening on that of a solar metallicity main sequence star of T_eff_=17000 K (B3-4 V). The functional dependence of the extinction curves on abundance is not as important in the Johnson-Cousins as in the Washington system. We compute new theoretical reddening vectors in both systems, and evaluate the size of the nonlinearity with extinction (Forbes effect).
Total interstellar extinction in UBVRI Star Star type number=1 MS = Main Sequence, RG = Red Giants (log(g)=2.5), SG = SuperGiants (i.e., the lowest surface gravity for that temperature in the Kurucz model family). --- [Fe/H] Metallicity Sun Teff Effective temperature K A(U)X Total interstellar extinction in U for airmass 1 (because U filter is defined by atmospheric cutoff) mag A(B)X Total interstellar extinction in B for airmass 1 (to allow calculation of U-B.) mag A(B) Total interstellar extinction in B for airmass 0 mag A(V) Total interstellar extinction in V for airmass 0 mag A(R) Total interstellar extinction in R for airmass 0 mag A(I) Total interstellar extinction in I for airmass 0 mag R(V) Ratio of total to differential extinction --- R(V)/R(V0) R(V0): same ratio as R(V) but for star with standard spectrum, i.e. T_eff=17000, log(g)=5.0, and [Fe/H]=0. --- Differential interstellar extinction in UBVRI Star Star type number=1 MS = Main Sequence, RG = Red Giants (log(g)=2.5), SG = SuperGiants (i.e., the lowest surface gravity for that temperature in the Kurucz model family). --- [Fe/H] Metallicity Sun Teff effective temperature K U-B (U-B) colour index mag E(U-B) differential interstellar extinction in (U-B) mag R1 E(U-B)/E(B-V) ratio --- B-V (B-V) colour index mag E(B-V) differential interstellar extinction in (B-V) mag R2 E(B-V)/E(B-V) ratio --- V-R (V-R) colour index mag E(V-R) differential interstellar extinction in (V-R) mag R3 E(V-R)/E(B-V) ratio --- R-I (R-I) colour index mag E(R-I) differential interstellar extinction in (R-I) mag R4 E(R-I)/E(B-V) ratio --- V-I (V-I) colour index mag E(V-I) differential interstellar extinction in (V-I) mag R5 E(V-I)/E(B-V) ratio --- Total interstellar extinction in CMT1T2 Star Star type number=1 MS = Main Sequence, RG = Red Giants (log(g)=2.5), SG = SuperGiants (i.e., the lowest surface gravity for that temperature in the Kurucz model family). --- [Fe/H] Metallicity Sun Teff Effective temperature K A(C) Total interstellar extinction in C for airmass 0 mag A(M) Total interstellar extinction in M for airmass 0 mag A(T1) Total interstellar extinction in T1 for airmass 0 mag A(T2) Total interstellar extinction in T2 for airmass 0 mag R(T2) Ratio of total to differential extinction --- R(T2)/R(V0) R(V0): same ratio as R(T2) but for star with standard spectrum, i.e. T_eff=17000, log(g)=5.0, and [Fe/H]=0.0 --- Differential interstellar extinction in CMT1T2 Star Star type number=1 MS = Main Sequence, RG = Red Giants (log(g)=2.5), SG = SuperGiants (i.e., the lowest surface gravity for that temperature in the Kurucz model family). --- [Fe/H] Metallicity Sun Teff effective temperature K C-M (C-M) colour index mag E(C-M) differential interstellar extinction in (C-M) mag R1 E(C-M)/E(M-T2) ratio --- M-T1 (M-T1) colour index mag E(M-T1) differential interstellar extinction in (M-T1) mag R2 E(M-T1)/E(M-T2) ratio --- T1-T2 (T1-T2) colour index mag E(T1-T2) differential interstellar extinction in (T1-T2) mag R3 E(T1-T2)/E(M-T2) ratio --- M-T2 (M-T2) colour index mag E(M-T2) differential interstellar extinction in (M-T2) mag R4 E(M-T2)/E(M-T2) ratio --- *Rational polynomial coefficients Filter Filters or quantity involved number=1 UB = U, U-B BR = B, B-R BV = V, B-V VI = V-I RV = R_V = A_V/E(B-V) CM = C, C-M M1 = M, M-T1 M2 = M-T2 R2 = R-T2 --- Band Quantity, e.g., filter or colour --- logg Surface gravity cm/s2 n_logg Lowest surface gravity model when there is no value for logg number=2 'm' means the lowest surface gravity model for that temperature in the Kurucz models, i.e., the SG=supergiants --- [Fe/H] Metallicity Sun num Numerator degree number=3 Degree of the numerator and the denominator of the best fitting rational polynomial found (in some cases a linear fit was chosen without searching for a higher order fit). The numerator always stars with a_0, so there is one more coefficient in the numerator than the degree. The denominator starts with b_1. --- den Denominator degree number=3 Degree of the numerator and the denominator of the best fitting rational polynomial found (in some cases a linear fit was chosen without searching for a higher order fit). The numerator always stars with a_0, so there is one more coefficient in the numerator than the degree. The denominator starts with b_1. --- MaxDev Largest deviation number=4 Largest deviation in extinction of the rational polynomial from any of the data points in the interstellar extinction table (dif* and tot*) for that fit, as returned by the Numerical Recipes routine 'ratlsq'. --- TCmin Lower boundary of the valid range of temperature colour for that fit number=5 For the ISM the TCs are B-V and M-T2. --- TCmax Upper boundary of the valid range of temperature colour for that fit number=5 For the ISM the TCs are B-V and M-T2. --- *Actual coefficients Band Quantity, e.g., filter or colour --- logg Surface gravity cm/s2 n_logg Lowest surface gravity model when there is no value for logg number=1 'm' means the lowest surface gravity model for that temperature in the Kurucz models, i.e., the SG=supergiants --- [Fe/H] Metallicity Sun a0 Coefficient a0 in the numerator --- a1 Coefficient a1 in the numerator --- a2 Coefficient a2 in the numerator --- a3 Coefficient a3 in the numerator --- a4 Coefficient a4 in the numerator --- a5 Coefficient a5 in the numerator --- a6 Coefficient a6 in the numerator --- a7 Coefficient a7 in the numerator --- a8 Coefficient a8 in the numerator --- b1 Coefficient b1 in the denominator --- b2 Coefficient b2 in the denominator --- b3 Coefficient b3 in the denominator --- b4 Coefficient b4 in the denominator --- b5 Coefficient b5 in the denominator --- b6 Coefficient b6 in the denominator --- b7 Coefficient b7 in the denominator --- Patricia Bauer CDS 1994 Sep 07 J_A+AS_109_293.xml Very low mass stars in the galactic cluster Praesepe J/A+AS/109/29 J/A+AS/109/29 Very low mass stars in Praesepe Very low mass stars in the galactic cluster Praesepe N C Hambly I A Steele M R S Hawkins R F Jameson Astron. Astrophys. Suppl. Ser. 109 29 1995 1995A&AS..109...29H astrometry low-mass open stars proper motions We present the results of a deep proper motion survey of a 19 square degree area of the Galactic open cluster Praesepe. Details of the astrometric and photometric reductions are given, along with the selection process for members.
Praesepe proper motion members Id Identification number --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec R(59F) R magnitude (590 nm) mag I(N) I magnitude (715 nm) mag Men Membership probability % Cross-identifications for proper motion members Id Identification number --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec KW27 Identification number in Klein-Wassink (1927) --- JC83 Identification number in Jones et al. (1983) --- JS91 Identification number in Jones et al. (1991) --- Patricia Bauer CDS 1994 Sep 07 J_A+AS_109_29.xml Heterochromatic extinction. I. Dependence of interstellar extinction on stellar temperature, surface gravity, and metallicity. J/A+AS/109/313 J/A+AS/109/313 Heterochromatic extinction. II. Heterochromatic extinction. I. Dependence of interstellar extinction on stellar temperature, surface gravity, and metallicity. W J Roberts E K Grebel Astron. Astrophys. Suppl. Ser. 109 313 1995 1995A&AS..109..313R atmospheric effects stars: fundamental parameters techniques: photometric In synthetic versions of two broadband photometric systems, Johnson-Cousins and Washington, we find the dependence of atmospheric extinction corrections on colour and on macro features in the spectra of stars, such as the Balmer jump, as parameterised by T_eff_, logg, and [Fe/H]. We use standard passbands, a mean atmospheric extinction law measured at ESO/La Silla, extended and modified by us, and the Kurucz library of synthetic spectra. The true broadband atmospheric extinction is far more complicated than any current reduction (transformation) methods consider. Hence all broadband magnitude systems are fundamentally unphysical - they contain not the extra-atmospheric magnitudes, but unobservable magnitudes whose relation to physical magnitudes is unknown, but may differ by 0.05mag or more for hot and cool stars. Hence, it is hazardous to compare them to any synthetic magnitude system derived from either synthetic spectra or spectral scans. These problems exist to a lesser degree in intermediate band systems, but narrow band systems are relatively immune from these complexities. We do not treat either kind of system here. If our results were incorporated into a photometric reduction program, and standard stars and program stars stars carefully selected by metallicity and luminosity class, a standard magnitude system could be established that would be directly comparable to synthetic systems. As a bonus, measurements of intrinsic flux variations at the millimagnitude level would become more secure. We describe our own operational photometric transformation program that incorporates only the linear part of the dependence on colour of atmospheric extinction. Our results and prescriptions are useful for aperture photoelectric photometry, but our implementation is aimed at CCD photometry of stellar populations.
Total atmospheric extinction in UBVRI Star Star type number=1 MS = Main Sequence, RG = Red Giants (log(g)=2.5), SG = SuperGiants (i.e., the lowest surface gravity for that temperature in the Kurucz model family). --- [Fe/H] Metallicity mag Teff Effective temperature K K(U)X Total atmospheric extinction coefficient in U for airmass 1 (because U filter is defined by atmospheric cutoff, see paper II) mag K(B)X Total atmospheric extinction coefficient in B for airmass 1 (to allow calculation of U-B.) mag K(B) Total atmospheric extinction coefficient in B for airmass 0 mag K(V) Total atmospheric extinction coefficient in V for airmass 0 mag K(R) Total atmospheric extinction coefficient in R for airmass 0 mag K(I) Total atmospheric extinction coefficient in I for airmass 0 mag Differential atmospheric extinction in UBVRI Star Star type number=1 MS = Main Sequence, RG = Red Giants (log(g)=2.5), SG = SuperGiants (i.e., the lowest surface gravity for that temperature in the Kurucz model family). --- [Fe/H] Metallicity mag Teff effective temperature K U-B (U-B) colour index mag K(U-B) Differential atmospheric extinction coefficient in (U-B) --- R1 K(U-B)/K(B-V) ratio --- B-V (B-V) colour index mag K(B-V) Differential atmospheric extinction coefficient in (B-V) --- R2 K(B-V)/K(B-V) ratio --- V-R (V-R) colour index mag K(V-R) Differential atmospheric extinction coefficient in (V-R) --- R3 K(V-R)/K(B-V) ratio --- R-I (R-I) colour index mag K(R-I) Differential atmospheric extinction coefficient in (R-I) --- R4 K(R-I)/K(B-V) ratio --- V-I (V-I) colour index mag K(V-I) Differential atmospheric extinction coefficient in (V-I) --- R5 K(V-I)/K(B-V) ratio --- Total atmospheric extinction in CMT1T2 Star Star type number=1 MS = Main Sequence, RG = Red Giants (log(g)=2.5), SG = SuperGiants (i.e., the lowest surface gravity for that temperature in the Kurucz model family). --- [Fe/H] Metallicity mag Teff Effective temperature K KC Total atm. ext. for C --- KM Total atm. ext. for M --- KT1 Total atm. ext. for T1 --- KT2 Total atm. ext. for T2 --- K51 Total atm. ext. for DDO 51 --- Differential atmospheric extinction in CMT1T2 Star Star type number=1 MS = Main Sequence, RG = Red Giants (log(g)=2.5), SG = SuperGiants (i.e., the lowest surface gravity for that temperature in the Kurucz model family). --- [Fe/H] Metallicity mag Teff effective temperature K C-M (C-M) colour index mag K(C-M) Differential atmospheric extinction coefficient for (C-M) --- R1 K(C-M)/K(M-T2) ratio --- M-T1 (M-T1) colour index mag K(M-T1) Differential atmospheric extinction coefficient for (M-T1) --- R2 K(M-T1)/K(M-T2) ratio --- T1-T2 (T1-T2) colour index mag K(T1-T2) Differential atmospheric extinction coefficient for (T1-T2) --- R3 K(T1-T2)/K(M-T2) ratio --- M-T2 (M-T2) colour index mag K(M-T2) Differential atmospheric extinction coefficient for (M-T2) --- R4 K(M-T2)/K(M-T2) ratio --- M-51 (M-DDO51) colour index mag K(M-51) Differential atmospheric extinction coefficient for (M-DDO51) --- R5 K(M-51)/K(M-T2) ratio --- *Rational polynomial coefficients Filter Filters or quantity involved number=1 UB = U, U-B BR = B, B-R BV = V, B-V VI = V-I CM = C, C-M M1 = M, M-T1 M2 = M-T2 --- Band Quantity, e.g., filter or colour --- logg Surface gravity cm/s2 n_logg Lowest surface gravity model when there is no value for logg number=2 'm' means the lowest surface gravity model for that temperature in the Kurucz models, i.e., the SG=supergiants --- [Fe/H] Metallicity mag num Numerator degree number=3 Degree of the numerator and the denominator of the best fitting rational polynomial found (in some cases a linear fit was chosen without searching for a higher order fit). The numerator always stars with a_0, so there is one more coefficient in the numerator than the degree. The denominator starts with b_1. --- den Denominator degree number=3 Degree of the numerator and the denominator of the best fitting rational polynomial found (in some cases a linear fit was chosen without searching for a higher order fit). The numerator always stars with a_0, so there is one more coefficient in the numerator than the degree. The denominator starts with b_1. --- MaxDev Largest deviation number=4 Largest deviation in extinction of the rational polynomial from any of the data points in the interstellar extinction table (dif* and tot*) for that fit, as returned by the Numerical Recipes routine 'ratlsq'. --- TCmin Lower boundary of the valid range of temperature colour for that fit number=5 For the atmospheric extinctions the TCs are V-I and M-T2. --- TCmax Upper boundary of the valid range of temperature colour for that fit number=5 For the atmospheric extinctions the TCs are V-I and M-T2. --- *Actual coefficients Band Quantity, e.g., filter or colour --- logg Surface gravity cm/s2 n_logg Lowest surface gravity model when there is no value for logg number=1 'm' means the lowest surface gravity model for that temperature in the Kurucz models, i.e., the SG=supergiants --- [Fe/H] Metallicity mag a0 Coefficient a0 in the numerator --- a1 Coefficient a1 in the numerator --- a2 Coefficient a2 in the numerator --- a3 Coefficient a3 in the numerator --- a4 Coefficient a4 in the numerator --- a5 Coefficient a5 in the numerator --- a6 Coefficient a6 in the numerator --- a7 Coefficient a7 in the numerator --- b1 Coefficient b1 in the denominator --- b2 Coefficient b2 in the denominator --- b3 Coefficient b3 in the denominator --- b4 Coefficient b4 in the denominator --- b5 Coefficient b5 in the denominator --- b6 Coefficient b6 in the denominator --- Patricia Bauer CDS 1994 Sep 07 J_A+AS_109_313.xml The UV properties of normal galaxies. II. The non-IUE data. J/A+AS/109/341 J/A+AS/109/341 UV properties of normal galaxies. II. The UV properties of normal galaxies. II. The non-IUE data. A Rifatto G Longo M Capaccioli Astron. Astrophys. Suppl. Ser. 109 341 1995 1995A&AS..109..341R J/A+AS/114/527 : Paper III Galaxies, photometry Photometry, ultraviolet catalogs galaxies: general galaxies: photometry In the last decade several satellite and balloon borne experiments have collected a large number of ultraviolet fluxes of normal galaxies measured through apertures of various sizes and shapes. We have homogenized this data set by deriving scale corrections with respect to IUE. In a forthcoming paper, these data will be used to derive standard luminosity profiles and total magnitudes.
List of normal galaxies with UV fluxes Name Identification --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec MType Morphological type --- Ref References --- UV magnitudes scaled to the IUE system Name Identification --- OAO(3320) OAO 3320A UV magnitude mag l_ANS(3300) limit flag on ANS(3300) --- ANS(3300) ANS 3300A UV magnitude mag OAO(2980) OAO 2980A UV magnitude mag TD1(2740) TD1 2740A UV magnitude mag l_ANS(2500) limit flag on ANS(2500) --- ANS(2500) ANS 2500A UV magnitude mag OAO(2460) OAO 2460A UV magnitude mag l_Astro(2420) limit flag on Astro(2420) --- Astro(2420) Astrobee 2420A UV magnitude mag TD1(2350) TD1 2350A UV magnitude mag Astro(2250) Astrobee 2250A UV magnitude mag l_ANS(2200) limit flag on ANS(2200) --- ANS(2200) ANS 2200A UV magnitude mag SCAP(2000) SCAP 2000A UV magnitude mag TD1(1950) TD1 1950A UV magnitude mag l_OAO(1800) limit flag on OAO(1800) --- OAO(1800) OAO 1800A UV magnitude mag l_ANS(1800) limit flag on ANS(1800) --- ANS(1800) ANS 1800A UV magnitude mag l_GUV(1560) limit flag on GUV(1560) --- GUV(1560) GUV 1560A UV magnitude mag n_GUV(1560) Note on GUV(1560) number=1 A * means that magnitude may be affected by overlap with other nearby and unresolved galaxies --- l_ANS(1550) limit flag ANS(1550) --- ANS(1550) ANS 1550A UV magnitude mag l_OAO(1550) limit flag on OAO(1550) --- OAO(1550) OAO 1550A UV magnitude mag TD1(1550) TD1 1550A UV magnitude mag Patricia Bauer CDS 1996 Mar 21 UNKNOWN UNKNOWN * 03-Oct-1994: table received at CDS from the author * 21-Mar-1996: 3 errors corrected, detected by Wayne Landsman <landsman@sorbet.gsfc.nasa.gov> J_A+AS_109_341.xml Catalogue of blue stragglers in open clusters J/A+AS/109/375 J/A+AS/109/375 Blue stragglers in open clusters Catalogue of blue stragglers in open clusters J Ahumada E Lapasset Astron. Astrophys. Suppl. Ser. 109 375 1995 1995A&AS..109..375A Clusters, open Stars, blue Stars, peculiar blue stragglers catalogs open clusters and associations: general An amount of 959 blue straggler candidates were selected from their position in the colour-magnitude diagram in 390 open clusters of all ages. A set of basic data is given for every cluster and blue straggler.
*Open cluster data Name Cluster designation --- RAh Right ascension 2000.0 h RAm Right ascension 2000.0 min DE- Declination sign --- DEd Declination 2000.0 deg DEm Declination 2000.0 arcmin E(B-V) Reddening mag (B-V)0 De-reddened turnoff colour mag log(Age) Decimal logarithm of the age in years [yr] ApDiam Apparent cluster diameter arcmin N2 Number of stars on the main sequence to two magnitudes below the turnoff --- Nbs Number of blue straggler candidates --- r_Name Photometry source(s) --- Note An asterisk indicates a note detailed in file notes.dat --- Blue stragglers in open clusters Name Cluster designation --- BluStrg Blue straggler designation (according to the referenced photometry) --- Class Blue straggler classification (following the criteria explained in the paper) --- Vmag V magnitude mag u_Vmag Uncertainty flag on V --- B-V B-V colour index mag u_B-V Uncertainty flag on B-V --- n_U-B Note on U-B. A 'd' stands for double --- U-B U-B colour-index mag u_U-B Uncertainty flag on U-B --- Phot Photometry in which the magnitudes are given. the type of photometry is defined by: pe = photoelectric, pg = photographic, CCD = charge-coupled-device --- r/R Relative radius of the blue straggler location --- r_Name Photometry source ---- Note An asterisk indicates a note detailed in file "notes.dat" --- Individual notes Name Cluster name, repeated when several lines --- Text Text of note --- References RefNo Reference number, repeated when several lines --- Text Reference as an ascii text. --- Patricia Bauer CDS 1994 Sep 28 UNKNOWN UNKNOWN * 28-Sep-1994: Prepared at CDS (Patricia Bauer) * 01-Mar-1999: notes & refs files reformatted. J_A+AS_109_375.xml Four-colour photometry of eclipsing binaries. XXVIIb. A photometric analysis of the (possible) Ap system AO Velorum J/A+AS/109/425 J/A+AS/109/425 AO Vel four-colour photometry Four-colour photometry of eclipsing binaries. XXVIIb. A photometric analysis of the (possible) Ap system AO Velorum J V Clausen A Gimnez C J Van Houten Astron. Astrophys. Suppl. Ser. 109 425 1995 1995A&AS..109..425C binaries: eclipsing stars: chemically peculiar stars: evolution stars: fundamental parameters stars: individual (AO Vel) *** No Description Available ***
Light curves: AO Vel - HD68631 in the Walraven system HJD Heliocentric Julian day d V-Vc V magnitude difference mag B-Bc B magnitude difference mag L-Lc L magnitude difference mag U-Uc U magnitude difference mag W-Wc W magnitude difference mag uvby observations: AO Vel - HR3203 instrumental system as in Paper I uvby observations: AO Vel - HR3327 instrumental system as in Paper I uvby observations: AO Vel - HR3327 new instrumental system HJD Heliocentric Julian day d ymag y magnitude mag (b-y) (b-y) colour index mag m1 m1 index mag c1 c1 index mag bmag b magnitude mag vmag v magnitude mag umag u magnitude mag Patricia Bauer CDS 1994 Sep 29 J_A+AS_109_425.xml Stellar models for a wide range of initial chemical compositions until helium burning I. From X=0.60 to X=0.80 for Z=0.02 J/A+AS/109/441 J/A+AS/109/441 Stellar models I. Stellar models for a wide range of initial chemical compositions until helium burning I. From X=0.60 to X=0.80 for Z=0.02 A Claret Astron. Astrophys. Suppl. Ser. 109 441 1995 1995A&AS..109..441C binaries: general stars: abundances stars: evolution stars: fundamental parameters stars: interiors New grids of stellar evolutionary models are presented for a wide range of initial hydrogen content around the solar composition. These compositions are (X, Z) = (0.80, 0.02), (0.70, 0.02) and (0.60, 0.02). Recent OPAL opacities with LS coupling and Grevesse composition were adopted, and Alexander's tables were used for lower temperatures. We consider models with core overshooting with {alpha}_ov_=0.20, and mixing length parameter l/H_p_=1.52 that seems to represent well double-lined eclipsing binary stars. Mass loss during the main sequence and in the red giant phase were taken into account. The nuclear network treats 14 isotopes and optionally the lithium burning to study its depletion in less massive models during pre main sequence evolution. The mass range covered goes from 1 up to 40M_{sun} _ and the more massive models were followed until helium burning. The main aim of the present series of papers is, besides the inclusion of the new opacities, to explore the effects on different outputs of the stellar models, of a change of the helium content at a given metallicity. We also present isochrones in the plane logg-logM which are very useful to compare the best parameters known for binary stars (masses and radii) with theoretical predictions. The internal structure constants for apsidal motion investigations are also presented
Grids of stellar evolutionary models logM Initial mass of the model solMass X X initial composition (H) --- Z Z initial composition --- Overshoot 0=without overshooting, 1= with overshooting --- Age Age of models yr log(L) Total luminosity solLum log(g) Surface gravity cm/s2 log(Teff) Effective temperature K log(k2) Apsidal motion constant (j=2) --- log(k3) Apsidal motion constant (j=3) --- log(k4) Apsidal motion constant (j=4) --- alpha alpha = -E_p x R/GM^2 --- beta Fractional gyration radius ---- Patricia Bauer CDS 1995 Mar 27 UNKNOWN UNKNOWN * 03-Oct-1994: Received at CDS * 27-Mar-1995: the caption of original tables 3 and 4 were interchanged (Antonio Claret dos Santos <aclaret@ll.iac.es>); the correction has been reported in "tables". J_A+AS_109_441.xml EROS catalogue of eclipsing binary stars in the bar of the Large Magellanic Cloud J/A+AS/109/447 J/A+AS/109/447 Eclipsing binaries EROS catalogue EROS catalogue of eclipsing binary stars in the bar of the Large Magellanic Cloud P Grison J -P Beaulieu J D Pritchard W Tobin R Ferlet A Vidal-Madjar J Guibert C Alard O Moreau F Tajahmady E Maurice L Prevot C Gry E Aubourg P Bareyre S Brehin M Gros M Lachieze-Rey B Laurent E Lesquoy C Magneville A Milsztajn L Moscoso F Queinnec C Renault J Rich M Spiro L Vigroux S Zylberajch R Ansari F Cavalier M Moniez Astron. Astrophys. Suppl. Ser. 109 447 1995 1995A&AS..109..447G binaries: eclipsing catalogs Magellanic Clouds Catalogue and photometry of eclipsing binary stars in the bar of the LMC obtained from observations in two colours made during 1991-92 by the French EROS project.
Be and Re photometry Name Name of star --- HJD Heliocentric moment of mid observation d Filt Filter (Be or Re) --- Mag EROS magnitude mag 79 certain or probable eclipsing binary stars in the bar of the LMC EROS EROS number starting at 10001 (eclipsing binaries) --- CCD Number of the detector on which the star fell --- x Harvard (x,y) coordinates of the star, accurate to about 3 arcsec number=1 Harvard system defined by Leanitt 1908, Ann. Harv. Coll. Obs, 60 No.4 arcsec y Harvard (x,y) coordinates of the star accurate to about 3 arcsec number=1 Harvard system defined by Leanitt 1908, Ann. Harv. Coll. Obs, 60 No.4 arcsec RAh Right ascension J2000.0 h RAm Right ascension J2000.0 min RAs Right ascension J2000.0 (accurate to 0.2-0.3 arcsec) s DE- Declination sign --- DEd Declination J2000.0 deg DEm Declination J2000.0 arcmin DEs Declination J2000.0 (accurate to 0.2-0.3 arcsec) arcsec To(p) The heliocentric Julian date of the designated primary minimum and its uncertainty. Where one eclipse is clearly deeper, it has been taken as the primary minimum. For some stars neither minimum is clearly deeper and the eclipse designated as primary is more or less arbitrary d e_To(p) rms uncertainty on To(p) d P Period of the system d e_P rms uncertainty on P d dTo(p)/dP A partial derivative indicating how much To(p) is affected by errors in P, where this is significant. -- Be(max) Approximate Be magnitudes at maximum light --- Re(max) Approximate Re magnitude at maximum light --- Rem Remarks: The section of the printed paper in which remarks are made about individual stars --- Times of secondary minima for obviously eccentric systems EROS EROS number --- To(s) Heliocentric Julian date of the secondary minimum for clearly eccentric systems d e_To(s) rms uncertainty for To(s) d dTo(s)/dP A partial derivative indicating how much To(s) is affected by errors in P, where this is significant. --- table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 Patricia Bauer CDS 1994 Oct 03 UNKNOWN UNKNOWN Transformations between EROS B and R magnitudes (Be and Re), and Johnson B and V magnitudes (Bj and Vj), and Cousins R magnitude (Rc). The transformations and the r.m.s. deviations of a single measure, sigma, are: Bj = Be + 0.46(Be - Re) sigma = 0.08 mag Vj = Be - 0.47(Be - Re) sigma = 0.07 mag Rc = Re + 0.07(Be - Re) sigma = 0.04 mag (Bj - Vj) = 0.92(Be - Re) sigma = 0.10 mag (Vj - Rc) = 0.49(Be - Re) sigma = 0.02 mag (Bj - Rc) = 1.37(Be - Re) sigma = 0.08 mag J_A+AS_109_447.xml A new photographic C-M diagram for NGC 4833 J/A+AS/109/479 J/A+AS/109/479 C-M diagram for NGC 4833 A new photographic C-M diagram for NGC 4833 N N Samus V Kravtsov M Pavlov G Alcaino W Liller Astron. Astrophys. Suppl. Ser. 109 479 1995 1995A&AS..109..479S globular clusters: individual (NGC 4833) Hertzsprung-Russell (HR diagram) A color-magnitude diagram for the galactic globular cluster NGC 4833, based on the photographic BV photometry of about 868 stars in a 12'x12' field with an automatic measuring machine, is presented. It reaches the cluster main sequence turn-off at V=~19.2mag; the difference in V magnitudes between the turn-off and the horizontal branch being normal.
Photographic photometry in NGC 4833 x x coordinate (increase to the west) mm y y coordinate (increase to the south) mm Vmag V magnitude mag B-V B-V color mag Tel Telescope code number=1 Telescope code c: Las Campanas Observatory 1 m telescope y: Cerro Tololo International Observatory Yale 1 m telescope e: European Southern Observatory 3.6 m telescope --- Identifications with previous works in NGC 4833 x x coordinate (increase to the west) mm y y coordinate (increase to the south) mm Id1 Identification with Menzies (1972) --- Id2 Identification with Alcaino (1971) --- UNKNOWN 24 Oct (End) Patricia Bauer [CDS] 1994 J_A+AS_109_479.xml A new photographic color-magnitude study of M 22 = NGC 6656 J/A+AS/109/487 J/A+AS/109/487 Color-magnitude study of M 22 A new photographic color-magnitude study of M 22 = NGC 6656 N Samus V Kravtsov M Pavlov G Alcaino W Liller Astron. Astrophys. Suppl. Ser. 109 487 1995 1995A&AS..109..487S globular clusters: individual (M 22) Hertzsprung-Russell (HR diagram) A new photographic C-M diagram for the globular cluster M 22 based on automatic plate measurements has been obtained. It reaches the main sequence turn-off at V=~17.1mag, (B-V)=~0.75.
Photographic photometry in M 22 x x coordinate (increase to the west) mm y y coordinate (increase to the south) mm Vmag V magnitude mag B-V B-V color mag Patricia Bauer CDS 1994 Oct 24 J_A+AS_109_487.xml Santiago 91, a right ascension catalogue of 3387 stars (equinox J2000) J/A+AS/109/501 J/A+AS/109/501 SANTIAGO 91, RA catalogue Santiago 91, a right ascension catalogue of 3387 stars (equinox J2000) G Carrasco P Loyola Astron. Astrophys. Suppl. Ser. 109 501 1995 1995A&AS..109..501C astrometry catalogs The positions in right ascension of 3387 stars belonging to the Santiago 67 Catalogue, observed with the Repsold Meridian Circle at Cerro Calan, National Astronomical Observatory, during the period 1989 to 1994, are given. The average mean square error of a position, for the whole Catalogue, is +/-0.009 s. The mean epoch of the catalogue is 1991.84.
SANTIAGO 91 catalogue Id Catalogue number --- DM Durchmusterung number --- Vmag Visual magnitude mag Sp Spectral type --- RAh Right ascension J2000.0 h RAm Right ascension J2000.0 min RAs Right ascension J2000.0 s EpRA Epoch-1900 of right ascension 0.01yr o_RAs Number of accepted observations in right ascension --- e_RAs rms uncertainty on right ascension 0.001s pmRA Annual proper motion in R.A. s/yr DE Declination J2000.0 deg Rem Remarks: FE: FK5 extension stars FEP: FK5 extension stars, parallax and radial velocity are taken P: parallax and radial velocity are taken PR: preceding star SQ: following star --- Patricia Bauer CDS 1994 Oct 06 J_A+AS_109_501.xml A redshift survey for faint galaxies towards voids of galaxies J/A+AS/109/537 J/A+AS/109/537 Redshift survey of faint galaxies A redshift survey for faint galaxies towards voids of galaxies U Hopp B Kuhm U Thiele K Birkle H Elsaesser Astron. Astrophys. Suppl. Ser. 109 537 1995 1995A&AS..109..537H galaxies: distances and redshifts galaxies: general large-scale structure of universe surveys We present the redshift and photometric data of a survey for intrinsically faint galaxies towards three nearby voids and the Hercules supercluster. The project is aimed at finding galaxies of absolute faint magnitudes or of low surface brightness within these voids. The selection of the voids and the search strategy for the galaxies are outlined. B and R magnitudes, major and minor diameters, as well as the morphology are determined. The diameter distribution of the galaxies is discussed. Optically measured redshifts of 174 galaxies are given. Most of the galaxies found show emission lines and late-type morphology. Several have low-surface brightness features. Our survey identified a higher percentage of nearby galaxies than magnitude or diameter limited surveys.
Photometry, diameters, types, and redshifts Sample Sample designation number=1 S1 = Sample 1, S2 = Sample2, BU = Back-up objects --- n_Name A 'N' indicates galaxies nearby to the subsample object with the same name which could be observed with the same slit setting --- Name Survey identification name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Bmag Total magnitude in B mag Rmag Total magnitude in R (Cousins) mag D Major semi-axis diameter arcsec d Minor semi-axis diameter arcsec z Redshift --- e_z rms uncertainty on z --- Type Type of the galaxy (see paper for explanation, if no normal Hubble convention, preceding L = low surface brightness, preceding P = peculiar) --- Identified lines in the spectra of the galaxies Sample Sample designation number=1 S1 = Sample 1, S2 = Sample2, BU = Back-up objects --- n_Name A 'N' indicates galaxies nearby to the subsample object with the same name which could be observed with the same slit setting --- Name Survey identification name --- z Redshift of the galaxy --- Line Usual astronomical abreviations to indicate the identified emission and/or absorption line; e.g. Ha = Halpha, G = G-band 4304 A; [OIII] = oxygen lines 4959, 5007, [OII] = oxygen doublet 3727, [NII] = [NII]6584, [SII] = [SII] 6716, 6731, etc. --- Patricia Bauer CDS 1994 Nov 07 J_A+AS_109_537.xml Stark broadening spectral lines of multicharged ions of astrophysical interest. XII. O IV and OV J/A+AS/109/551 J/A+AS/109/551 Stark broadening. XII. OIV & OV Stark broadening spectral lines of multicharged ions of astrophysical interest. XII. O IV and OV M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 109 551 1995 1995A&AS..109..551D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar MgI lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles molecular data Using a semiclassical approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 5 O IV and 19 O V multiplets.
Stark broadening parameters due to e-, p- and He III-impacts for O IV and O V N Perturber density cm-3 El Element --- Tr Transition --- Lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We See note number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de See note number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- de Shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp See note number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- Wp FWHM for proton impacts (2) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp See note number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dp Shift for proton impacts (3) number=5 Values for N V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ See note number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ See note number=4 An asterisk in this column indicates that 0.1 < N V < 0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dHe++ Shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1994 Dec 14 Sylvie Sahal-Brechot & Milan S. Dimitrijevic J_A+AS_109_551.xml The EXOSAT GSPC iron line catalog. J/A+AS/109/9 J/A+AS/109/9 EXOSAT GSPC iron line catalog The EXOSAT GSPC iron line catalog. M Gottwald A N Parmar A P Reynolds N E White A Peacock B G Taylor Astron. Astrophys. Suppl. Ser. 109 9 1995 1995A&AS..109....9G catalogs X-rays: general We report on the global properties of the Fe feature seen in the 6-7keV spectra of X-ray sources observed with the EXOSAT Gas Scintillation Proportional Counter (GSPC). Of a total of 431 spectra extracted from the EXOSAT archive, 205 required the addition of a Gaussian emission line to the continuum spectrum in order to obtain satisfactory fits. The majority of these sources are X-ray binaries. The best fit line properties are given for each of these spectra as well as being summarized by source class. For the 226 spectra which did not require the addition of an emission feature, upper limit equivalent widths for narrow and broad lines are presented.
EXOSAT
Data (table1, table2 and table3) Name Source name ---- Type Source type number=1 The source classification according to Gottwald et al (1994). The sources are AGN (active galactic nuclei), LMXRB (low mass X-ray binaries), HMXRB (high mass X-ray binaries), CV (cataclysmic variables), SNR (supernova remnants), CG (clusters of galaxies) and UNID (unidentified sources). ---- Time Start time number=2 the start time is given in seconds since 1980 January 1.0 (to one second precision) s Obs Duration of observation s RAdeg Right ascension deg DEd Declination deg 3-10keV 3-10 keV count rate ct/s Fit Type of fit (LINE or UPPER for upper-limit) --- Le Line energy keV e(Le)u Error in line energy (upper interval) keV e(Le)l Error in line energy (lower interval) keV FWHM Line FWHM (0.0 indicates no fit made) keV e(FWHM)u Error in line FWHM (upper interval) keV e(FWHM)l Error in line FWHM (lower interval) keV Flux Line flux (0.00 indicates no fit) 0.001ph/cm2/s e(FLux)u Error in line flux (upper interval) 0.001ph/cm2/s e(FLux)u Error in line flux (lower interval) 0.001ph/cm2/s EW Line EW ("0" = upper limit fit) eV Fluxcont1 Continuum flux for line fit 10-13W/m2 Model1 Best model for a line fit number=3 The codes have the following meanings. -------- = No line fit made BB = Blackbody CPL = Cutoff power law L = Line THB = Thermal Bremsstrahlung E = Edge --- Chi Reduced Chi squared for fit --- sig Significance of the fit (in sigma) --- Fluxcont2 Continuum flux for upper limit fit 10-13W/m2 Model2 Best model for continuum fit number=3 The codes have the following meanings. -------- = No line fit made BB = Blackbody CPL = Cutoff power law L = Line THB = Thermal Bremsstrahlung E = Edge --- EWnl Upper limit EW for narrow line eV EWbl Upper limit EW for broad line eV Patricia Bauer CDS 1994 Nov 10 UNKNOWN UNKNOWN The EXOSAT GSPC iron line catalog is available as an online database within the EXOSAT archive maintained at ESTEC in Noordwijk, Holland. The archive can be reached via either decnet or internet: set h exosat (username "XRAY") telnet exosat.estec.esa.nl (username "XRAY"). Access the GSPC iron line database (known as FELINE) by using the BROWSE program available within the EXOSAT system. Contact A.P. Reynolds (areynold@exosat.estec.esa.nl) with queries J_A+AS_109_9.xml Gaseous and stellar components in mixed pairs of galaxies. I. The data. J/A+AS/110/131 J/A+AS/110/131 Mixed pairs of galaxies. I. Gaseous and stellar components in mixed pairs of galaxies. I. The data. R Rampazzo L Reduzzi J W Sulentic R Madejsky Astron. Astrophys. Suppl. Ser. 110 131 1995 1995A&AS..110..131R galaxies: elliptical and lenticular, cD galaxies: interactions galaxies: kinematics and dynamics galaxies: photometry galaxies: spiral We present data from a kinematic and photometric study of six mixed pairs. High resolution rotation and velocity dispersion curves, for both gas and stellar components, are presented. Slit orientations were along the major axis of the spiral and, in most of the cases, along the line connecting the galaxy nuclei. B and V luminosity and geometrical profiles and photometric parameters including effective radius and disk scale length are also presented.
cz from emission lines Name Galaxy name --- PA Position angle deg Rad Radius arcsec H{alpha} cz from H{alpha} emission line km/s [NII] cz from [NII] emission line km/s [SII] cz from [SII] emission line km/s H{beta} cz from H{beta} emission line km/s n1[OIII] cz from n1[OIII] emission line km/s n2[OIII] cz from n2[OIII] emission line km/s cz and velocity dispersion for absorption and emission lines Name Galaxy name --- PA Position angle deg Rad Radius arcsec cz(a) cz from absorption line km/s e_cz(a) rms uncertainty on cz(a) km/s sigma Absorption line velocity dispersion km/s e_sigma rms uncertainty on sigma km/s cz(e) cz from emission line (only for NGC 5953) km/s B photometry Name Galaxy name --- a Semi-major axis arcsec muB B luminosity profile mag/arcsec+2 eB Ellipticity (geometrical parameter) --- tB Twisting (geometrical parameter) --- V photometry Name Galaxy name --- a Semi-major axis arcsec muV V luminosity profile mag/arcsec+2 eV Ellipticity (geometrical parameter) --- tV Twisting (geometrical parameter) --- table4a.tex Tex version of table4 (first part) table4b.tex LaTeX version of table4 (second part) table6.tex LaTeX version of table6 Patricia Bauer CDS 1994 Nov 18 J_A+AS_110_131.xml Radial velocities. VII. Ground based measurements for HIPPARCOS. J/A+AS/110/177 J/A+AS/110/177 Radial velocities. VII. Radial velocities. VII. Ground based measurements for HIPPARCOS. M Duflot C Fehrenbach C Mannone R Burnage V Genty Astron. Astrophys. Suppl. Ser. 110 177 1995 1995A&AS..110..177D Radial velocities Galaxy: kinematics and dynamics techniques: radial velocities We publish 734 radial velocities of stars distributed in 28 fields of 4x4deg. We continue the PPO series (Fehrenbach et al. 1987; Duflot et al. 1990 and 1992), using the Fehrenbach objective prism method.
Mean radial velocity data Field PPO stellar field number --- HD HD number --- BD BD number --- Sp Spectral type --- No Number of the comparison star --- Mvis Visual magnitude mag Mphot Photographic magnitude mag RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin RV Radial velocity km/s e_RV rms uncertainty on RV km/s o_RV Number of measurements --- Bin An '*' means visual binary --- Individual radial velocity data Name HD or BD number --- Obs Observation date in julian days d RV Radial velocity km/s Field PPO stellar field number --- Patricia Bauer, Francois Ochsenbein CDS 1995 Jan 27 UNKNOWN UNKNOWN * 21-Apr-1995: a few errors which have been found in the paper version were corrected; these concern in table2 Field 1815: BD 16 3485 and BD 17 3536 Field 2015: HD 191162 and HD 191262 J_A+AS_110_177.xml Kinematical observations of pairs of galaxies. J/A+AS/110/19 J/A+AS/110/19 Kinematical observations of pairs of galaxies Kinematical observations of pairs of galaxies. E Davoust S Considere Astron. Astrophys. Suppl. Ser. 110 19 1995 1995A&AS..110...19D Galaxies, spectra Redshifts galaxies: distances and redshifts galaxies: elliptical and lenticular, cD galaxies: kinematics and dynamics galaxies: spiral We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.
Description of the observing runs No Number of the observing run --- Obs Observer number=1 JLN = Jean-Luc Nieto, PhP = Philippe Prugniel, ED = Emmanuel Davoust, SC = Suzanne Considere, OB = Olivier Bienayme --- Date Period of observation --- Disp Dispersion 0.1nm/mm sw Slit width arcsec nS Number of spectra --- nG number of galaxies --- Spectroscopic observations of galaxy pairs Name Galaxy name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec n_DEd Note on declination number=1 * = accurate coordinates (error smaller than 10arcsec) or accurate magnitude (error smaller than 0.3mag) --- Vmag V magnitude mag n_Vmag Note on V magnitude number=1 * = accurate coordinates (error smaller than 10arcsec) or accurate magnitude (error smaller than 0.3mag) --- Sep Separation arcsec u_Sep Uncertainty flag on Sep --- PA Position angle deg n_PA Orientation of the PA data --- RV1(e) e when radial velocity of emission line --- RV1 Radial velocity km/s n_RV1 Note on radial velocity number=1 * = accurate coordinates (error smaller than 10arcsec) or accurate magnitude (error smaller than 0.3mag) --- e_RV1 rms uncertainty on RV1 km/s u_RV1 Uncertainty flag on RV1 --- nRV1 Orientation of the RV1 data --- RV2(e) e when radial velocity of emission line --- RV2 Radial velocity km/s n_RV2 Note on Radial velocity number=1 * = accurate coordinates (error smaller than 10arcsec) or accurate magnitude (error smaller than 0.3mag) --- e_RV2 rms uncertainty on RV2 km/s u_RV2 Uncertainty flag on RV@ --- No Observing run (see table1) number=2 The references to velocities in the literature (last column) are the following: KNF = Kollatschny et al. (1986A&A...163...31K). M90 = Madejsky (1990). PDN = Prugniel et al. (1989A&A...222....5P). PGC = Paturel et al. (1989), Cat. <VII/119> S90 = Smith et al. (1990ApJ...356..399S). T85 = Tonry (1985AJ.....90.2431T). K followed by a number is the corresponding pair in Karachentsev (1987), see Cat. <VII/77> --- Characteristics of emission-line spectra of galaxies Name Galaxy name --- EL Identified emission lines --- Class Class number=1 1: HII, according to the line ratios of Kollatschny et al. (1986) 2: the activity was determined from [OI]/Halpha and [OIII]/Hbeta. 3: the emission is of circum-nuclear type, located about +/-4arcsec from the center; there is no emission in the very center of the galaxy. --- Central velocity dispersions of galaxy pairs Name Galaxy name --- n_sigma1 Orientation for sigma1 data --- sigma1 Central velocity dispersion of the brighter component km/s e_sigma1 rms uncertainty on sigma1 km/s n_sigma2 Orientation of the fainter component --- sigma2 Central velocity dispersion of the fainter component km/s e_sigma2 rms uncertainty on sigma2 km/s Ref run/dispersion or references number=1 BN90 = Bender & Nieto (1990A&A...239...97B); B94 = Borne et al. (1994ApJ...435...79B); D87 = Davies et al, (1987ApJS...64..581D); F89 = Franx et al, (1989ApJ...344..613F); MK85 = Malumuth & Kirshner (1985ApJ...291....8M); S90 = Smith et al. (1990ApJ...356..399S); T85 = Tonry (1985AJ.....90.2431T); TD81 = Tonry & Davis (1981) --- Patricia Bauer CDS 1997 Jan 21 Emmanuel Davoust <davoust@srvdec.obs-mip.fr> UNKNOWN UNKNOWN * 28-May-1996: First version; an error in the conversion of table2 resulted in missing Sep, PA and RV data * 21-Jan-1997: table2 corrected. J_A+AS_110_19.xml The CCD photometry of the globular cluster Palomar 1. J/A+AS/110/1 J/A+AS/110/1 CCD photometry of Pal 1 The CCD photometry of the globular cluster Palomar 1. J Borissova N Spassova Astron. Astrophys. Suppl. Ser. 110 1 1995 1995A&AS..110....1B Clusters, globular Photometry, CCD globular clusters: individual (Pal 1) Hertzsprung-Russell (HR diagram) A CCD photometry of the halo cluster Palomar 1 is presented in the Thuan-Gunn photometric system. The principal sequences of the color-magnitude diagrams are delineated in different spectral bands. The color- magnitude diagrams of the cluster show a well defined red horizontal branch, a subgiant branch and a main-sequence down to about two magnitudes below the main sequence turnoff. The giant branch is absent and the brightest stars are the horizontal branch stars. The age of the cluster determined by comparison with the isochrones of Bell & VandenBerg (1987ApJS...63..335B) is consistent with an age in the interval 12-14Gyr. A distance modulus of (m-M)_g0_=15.38+/-0.15 magnitude and E(g-r)=0.16 has been derived. An estimate of the cluster structural parameters such as core radius and concentration parameter gives r_c_=1.5pc and c=1.46. A mass estimate of 1.1x10^3^M_{sun}_ and a mass-to-light ratio of 1.79 have been obtained using King's (1966AJ.....71...64K) method. The morphology of color-magnitude diagrams allows Pal 1 to be interpreted as probably a globular cluster rather than an old open one. For a description of the uvgr photometric system, see e.g. <GCPD/38>
Pal 1 C 0325+794 03 33 23.0 +79 34 50
CCD photometry of Pal 1 ID Identification number (Palomar 1 BS NNN) --- Xpos X position number=1 1pix=0.8arcsec. X increasing from North to South, Y from East to West. pix Ypos Y position number=1 1pix=0.8arcsec. X increasing from North to South, Y from East to West. pix gmag g magnitude mag rmag r magnitude mag imag i magnitude mag zmag z magnitude mag James Marcout, Patricia Bauer CDS 1997 Jun 12 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_110_1.xml Penetrating the "zone of avoidance". I. A compilation of optically identified extragalactic objects within |b| <= 5 J/A+AS/110/269 J/A+AS/110/269 Galaxies in the "zone of avoidance". I. Penetrating the "zone of avoidance". I. A compilation of optically identified extragalactic objects within |b| <= 5 R Weinberger W Saurer R Seeberger Astron. Astrophys. Suppl. Ser. 110 269 1995 1995A&AS..110..269W J/A+AS/117/1 : Part II, 180<l<240 J/A+AS/117/369 : Part III, 120<l<130, |b|<10 Cross identifications Galaxy catalogs catalogs dust, extinction galaxies: general large-scale structure of universe We present a compilation of hopefully all published galaxies and quasars that were ever optically identified within |b|=<5deg. We present 2304 objects and list (and discuss), in addition to their (often considerably improved) coordinates, the best available morphological type, optical maximum diameters in the red, up-to-date heliocentric radial velocities, references to the papers where a specific object was first optically identified and results of cross-checks with the IRAS point source catalogue.
A compilation of optically identified and published galaxies within l=0-360; |b|<5 Name Zone Of Avoidance Galaxy Name of the galaxy in galactic coordinate --- CrossId Cross-identification --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin RAh2000 Right ascension 2000 h RAm2000 Right ascension 2000 min RAs2000 Right ascension 2000 s DE-2000 Declination sign --- DEd2000 Declination 2000 deg DEm2000 Declination 2000 arcmin MType Morphological type --- Diam Optical maximum diameter (red wavelength region) arcmin u_Diam uncertainty flag on Diam --- HRV Heliocentric radial velocity km/s n_HRV if "*" see discussion in the text --- Ref Reference of the paper where for the first time an object was optically identified as a galaxy (quasar), see Note number=1 References to the table: 01 Mayall N.U., 1935, PASP 47, 317 02 Boehm-Vitense E., 1956, PASP 68, 430 =1956PASP...68..430B 03 Vorontsov-Velyaminov B.A., Krasnogorskaja A., 1962, Morphological Catalogue of Galaxies I (catalog <VII/62>) 04 Zwicky F., Herzog E., 1963, Catalogue of Galaxies and of Clusters of Galaxies Vol II, California Institute of Technology (catalog <VII/49>) 05 Vorontsov-Velyaminov B.A., Arhipova V.P., 1963, Morphological Catalogue of Galaxies III (catalog <VII/62>) 06 Bolton J.G., Gardner F.F., Mackey M.B., 1964, Austr. J. Phys. 17, 340 07 Vorontsov-Velyaminov B.A., Arhipova V.P., 1964, Morphological Catalogue of Galaxies II (catalog <VII/62>) 08 Sandage A., Veron P., Wyndham J.D., 1965, ApJ 142, 1307 09 Zwicky F., 1965, Seven Privately Circulated Lists 10 Wyndham J.D., 1966, ApJ 144, 459 11 Bolton J.G., Ekers J., 1966, Aust. J. Phys. 19, 275 12 Bolton J.G., Ekers J., 1966, Aust. J. Phys. 19, 559 13 Bolton J.G., Ekers J., 1966, Aust. J. 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Ann. 6 (catalog <VII/26>) 22 FitzGerald M.P., 1974, A&A 31, 467 (=1974A&A....31..467F) 23 Vorontsov-Velyaminov B.A., Arhipova V.P., 1974, Morphological Catalogue of Galaxies V (Catalog <VII/100>) 24 Adgie R.L., Palmer H.P., Penston M.V., 1975, MNRAS 170, 31p =1975MNRAS.170p..31A 25 Riley J.M., Pooley G.G., 1975, Mem. R. Astron. Soc. 80, 105 26 Holmberg E.B., Lauberts A., Schuster H.-E., West R.M., 1975, A&AS 22, 327 (=1975A&AS...22..327H) 27 Sandage A., 1975, PASP 87, 853 28 Weinberger R., Elsaesser H., Beetz M., Birkle K., 1976, A&A 48, 327 29 Mebold U., Goss W.M., Woerden H. van, Freeman K.C., 1976, Proc. Astron. Soc. 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Observation of spirals in Virgo.III J/A+AS/110/279 J/A+AS/110/279 Spirals in Virgo. III. Optical studies of galaxies in cluster. Observation of spirals in Virgo.III M Sperandio G Chincarini R Rampazzo R De Souza Astron. Astrophys. Suppl. Ser. 110 279 1995 1995A&AS..110..279S galaxies: clusters: individual (Virgo cluster) galaxies: kinematics and dynamics galaxies: spiral We present the analysis of the rotation curves of a sample of 32 spiral galaxies derived from the spectroscopic observations of a sample of 47 galaxies.
Line-of-sight velocities in H{alpha} Name Galaxy name --- PA Position angle deg Samp Sample name number=1 CdS: Chincarini G. and de Souza R. 1985 A&A, 153, 218; RS: Rampazzo R. and Sperandio M. obtained with the ESO 1.5m telescope in 1989. --- Rad Halpha radius arcsec Vel Halpha velocity km/s Line-of-sight velocities in N[II] Name Galaxy name --- PA Position angle deg Samp Sample name (see Note (1) above) --- Rad N[II] radius arcsec Vel N[II] velocity km/s tab3.tex LaTeX version of table3 (first part) tab3cont.tex LaTeX version of table3 (second part) Patricia Bauer CDS 1994 Nov 03 J_A+AS_110_279.xml New proper motion determination of Luyten catalogue stars (LTT) south of declination -40deg and right ascension between 16h and 24h. J/A+AS/110/27 J/A+AS/110/27 Proper motion of LTT stars New proper motion determination of Luyten catalogue stars (LTT) south of declination -40deg and right ascension between 16h and 24h. H Wroblewski C Torres Astron. Astrophys. Suppl. Ser. 110 27 1995 1995A&AS..110...27W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/78/231 : Dec<-40, 0<RA<4h30, stars 1 to 144 (Wroblewski+ 1989) J/A+AS/91/129 : Dec<-40, 0<RA<4h30, stars 145 to 521 (Wroblewski+ 1991) J/A+AS/105/179 : Dec<-40, 16<RA<24h, stars 522 to 1069 (Wroblewski+ 1994) J/A+AS/115/481 : -30<Dec<-5, 0<RA<9h, stars 1070 to 1563 (Wroblewski+ 1996) J/A+AS/83/317 : LTT stars, Dec<-40, 0<RA<4h30 (Wroblewski+ 1990) J/A+AS/92/449 : LTT stars, Dec<-40, 4h30<RA<16h (Wroblewski+ 1992) Luyten W.J. 1957, A Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motions Exceeding 0.2 arcsec Annualy (The Lund Press, Minneapolis, Minnesota). Luyten W.J. 1979, LHS Catalogue, University of Minnesota, Minneapolis, Minnesota. (Cat. <I/87>) Proper motions astrometry stars: kinematics Data are given for 285 LTT stars found on 23 areas, covering 25 square degrees each, south of declination -40deg and right ascension between 16h and 24h. Four stars present differences in proper motion greater than 0.10 arcsec, eleven present differences in position angle >20deg and one presents those differences in both values.
Positions and relative proper motions ID Correlative number --- LTT Star number in Luyten's catalogue (LTT) --- Location Location numbers where the first digits refer to the area number and the other refer to the star number in the area --- Vmag V magnitude mag RAh Right ascension B1950.0 h RAm Right ascension B1950.0 min RAs Right ascension B1950.0 s DE- Declination sign --- DEd Declination B1950.0 deg DEm Declination B1950.0 arcmin DEs Declination B1950.0 arcsec RAh2000 Right ascension J2000.0 h RAm2000 Right ascension J2000.0 min RAs2000 Right ascension J2000.0 s DE-2000 Declination sign --- DEd2000 Declination J2000.0 deg DEm2000 Declination J2000.0 arcmin DEs2000 Declination J2000.0 arcsec pm Annual proper motion (J2000.0) arcsec/yr e_pm rms uncertainty on pm arcsec/yr pmPA Position angle (J2000.0) of proper motion deg Dpm Comparison of our proper motions with the LTT proper motions in sense LTT minus ours. arcsec Remark Remarks number=1 The annual proper motions, and the position angles, given in table1 are the means of the two values obtained from the plate pairs; 19 LTT stars were common to the overlapped areas mentioned above. For them, the results given in table1 (indicated by 4 in column Remark) correspond to the means of the values obtained from four plate pairs. One proper-motion star is common to three overlapped areas, for it the results given in the same table (indicated by 6 in column Remark) correspond to the mean of the values obtained from six plate pairs. It can be seen that most proper motions given in LTT are larger than those determined by us. It is important to point out that stars 121 (LTT 8146), 137 (LTT 8323), 146 (LTT 8382), 201 (LTT 8890) and 218 (LTT 8990) show considerable differences (>0.10"). On the other hand, stars 9 (LTT 6751), 37 (LTT 7432), 41 (LTT 7459), 59 (LTT 7572), 65 (LTT 7619), 105 (LTT 8034), 133 (LTT 8285), 137 (LTT 8323), 144 (LTT 8367), 194 (LTT 8859), 223 (LTT 9027) and 260 (LTT 9645) identified by (1) in column Remarks, show values of position angles that differ by more than 20deg. It is also important to note that the stars 27 (LTT 7391), 273 (LTT 9783) and 276 (LTT 9792), indicated with (2) in column Remarks, were not found in the position given by Luyten's Catalog. The stars LTT 7365, LTT 7367, LTT 7371, LTT 7899, LTT 7973, LTT 8213 and LTT 8388 were not found in our plates; from those stars LTT 7973 has the same name (-51 12417) than LTT 7986. We could not resolve in our plates the stars LTT 7510 and LTT 8855 from their companion stars LTT 7509 and LTT 8854 respectively. The star LTT 9141 appear in our plates as a double star. --- Patricia Bauer CDS 1994 Nov 10 J_A+AS_110_27.xml L'astrolabe du ROA. Observations du Soleil en 1992. Observations of the Sun at ROA astrolabe in 1992. J/A+AS/110/351 J/A+AS/110/351 Sun observations in 1992 L'astrolabe du ROA. Observations du Soleil en 1992. Observations of the Sun at ROA astrolabe in 1992. M Sanchez F Parra M Soler R Soto Astron. Astrophys. Suppl. Ser. 110 351 1995 1995A&AS..110..351S astrometry Sun: fundamental parameters Sun: general The results of an observational campaign of the Sun are reported.
UT0-UTC and Delta{phi} values following IERS (International Earth Rotation System) MJD Modified Julian day d Dphi Variation of local latitude arcsec UT0-UTC UT0-UTC value s Results for 1992 solar campaign at 60deg height Date Date (Month, day) --- MJD Modified Julian day d Obs Observers number=1 Observators: 6: M. Sanchez; 7: F. Parra; 13: R. Soto; 16: M. Soler --- BSE East upper limb passage observation residual arcsec n_BSE Note on BSE number=2 A '*' signifies that the limbs are not observed (clouds, errors, etc.) --- BIE East lower limb passage observation residual arcsec n_BIE Note on BIE number=2 A '*' signifies that the limbs are not observed (clouds, errors, etc.) --- BIW West lower limb passage observation residual arcsec n_BIW Note on BIW number=2 A '*' signifies that the limbs are not observed (clouds, errors, etc.) --- BSW West upper limb passage observation residual arcsec n_BSW Note on BSW number=2 A '*' signifies that the limbs are not observed (clouds, errors, etc.) --- dRA Offset in right ascension s e_dRA rms uncertainty on dRA s Y Y=Delta(z) +Delta(delta)cos(S) number=3 Y=Delta(z) + Delta(delta)cos(S) where, Delta(z) is the correction in zenithal distance, Delta(delta) is the correction in declination and S is the angle at the celestial object arcsec DS Correction in calculated apparent demi-diameter arcsec e_DS rms uncertainty on DS arcsec S Semi-diameter rapported to the astronomical unit arcsec table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 Patricia Bauer CDS 1994 Dec 13 J_A+AS_110_351.xml Sourthern binary galaxies. I. A sample of isolated pairs. J/A+AS/110/371 J/A+AS/110/371 Sourthern binary galaxies. I. Sourthern binary galaxies. I. A sample of isolated pairs. D S L Soares R E De Souza R R De Carvalho T C Couto Da Silva Astron. Astrophys. Suppl. Ser. 110 371 1995 1995A&AS..110..371S catalogs galaxies: interactions galaxies: luminosity function, mass function A catalogue of binary galaxies with 621 pairs has been determined by applying a surface density enhancement procedure to The Surface Photometry Catalogue of the ESO-Uppsala Galaxies. The method does not require any redshift information. An additional restriction, based on objective criteria that take into account the completeness of the source catalogue, led to a sample of 189 isolated pairs which are listed. We have obtained the optical luminosity function of binary galaxies in the catalogue, from which we estimate that the luminosity density of galaxies in binaries is ~4% of that found for field galaxies. The general properties of our sample are similar to those from CPG and CMG.
ESO-LV Binary list Name Pair identification in the main list --- Primary Identification of primary --- RAh1 Right ascension 1950 of the primary h RAm1 Right ascension 1950 of the primary min RAs1 Right ascension 1950 of the primary s DE-1 Declination sign --- DEd1 Declination 1950 of the primary deg DEm1 Declination 1950 of the primary arcmin DEs1 Declination 1950 of the primary arcsec Bmag1 Blue magnitude of the primary mag Type1 Numerical type of the primary --- RV1 Radial velocity of the primary km/s Secondary Identification of secondary --- RAh2 Right ascension 1950 of the secondary h RAm2 Right ascension 1950 of the secondary min RAs2 Right ascension 1950 of the secondary s DE-2 Declination sign --- DEd2 Declination 1950 of the secondary deg DEm2 Declination 1950 of the secondary arcmin DEs2 Declination 1950 of the secondary arcsec Bmag2 Blue magnitude of the secondary mag Type2 Numerical type of the secondary --- RV2 Radial velocity of the secondary km/s Sep Separation arcsec Prob Probability parameter % Com Comments --- Patricia Bauer CDS 1994 Dec 14 J_A+AS_110_371.xml High order f and g power series for orbit determination. J/A+AS/110/411 J/A+AS/110/411 Orbit determination f & g power series High order f and g power series for orbit determination. J Bem B Szczodrowska-Kozar Astron. Astrophys. Suppl. Ser. 110 411 1995 1995A&AS..110..411B celestial mechanics, stellar dynamics methods: numerical solar system: general The table of coefficients and exponents of the power series f and g up to derivatives of the 20-th order is the main achievement of this paper. The accuracy of the calculation of orbits has been tested by tracing the motion of all planets of the solar system.
Coefficients and exponents n Order of derivative -- L+L' Number of terms belonging to the derivative --- R" Coefficient R" in next L+L' lines number=1 To solve the Newtonian equation, d^2^r/dt^2^=-ur, in Taylor's series form r={sum(n>=0)}[d^0^r/dt^0^(tau^n^/n!)], and after introducing Lagrangian variables u, p and q; the successive terms of Taylor's series of order n take the form: tau^n^[r_0_{sum(1,L)}(R_L_.u^i^.p^j^.q^k^) + dr_0_/dt{sum(1,L')}(R_L'_.u^i^.p^j^.q^k^)]/n! (5) R are integers numbers, R'=R/n! and R"=R'/(n+1) --- i Exponent i of each term number=1 To solve the Newtonian equation, d^2^r/dt^2^=-ur, in Taylor's series form r={sum(n>=0)}[d^0^r/dt^0^(tau^n^/n!)], and after introducing Lagrangian variables u, p and q; the successive terms of Taylor's series of order n take the form: tau^n^[r_0_{sum(1,L)}(R_L_.u^i^.p^j^.q^k^) + dr_0_/dt{sum(1,L')}(R_L'_.u^i^.p^j^.q^k^)]/n! (5) R are integers numbers, R'=R/n! and R"=R'/(n+1) --- j Exponent j of each term number=1 To solve the Newtonian equation, d^2^r/dt^2^=-ur, in Taylor's series form r={sum(n>=0)}[d^0^r/dt^0^(tau^n^/n!)], and after introducing Lagrangian variables u, p and q; the successive terms of Taylor's series of order n take the form: tau^n^[r_0_{sum(1,L)}(R_L_.u^i^.p^j^.q^k^) + dr_0_/dt{sum(1,L')}(R_L'_.u^i^.p^j^.q^k^)]/n! (5) R are integers numbers, R'=R/n! and R"=R'/(n+1) --- k Exponent k of each term number=1 To solve the Newtonian equation, d^2^r/dt^2^=-ur, in Taylor's series form r={sum(n>=0)}[d^0^r/dt^0^(tau^n^/n!)], and after introducing Lagrangian variables u, p and q; the successive terms of Taylor's series of order n take the form: tau^n^[r_0_{sum(1,L)}(R_L_.u^i^.p^j^.q^k^) + dr_0_/dt{sum(1,L')}(R_L'_.u^i^.p^j^.q^k^)]/n! (5) R are integers numbers, R'=R/n! and R"=R'/(n+1) --- fg Term of the serie, 1 for f, 2 for g --- Patricia Bauer CDS 1994 Dec 12 J_A+AS_110_411.xml The 7C survey of radio sources at 151 MHz. A 418-square-degree region centred at RA = 17h, Dec = +65deg J/A+AS/110/419 J/A+AS/110/419 7C survey of radio sources The 7C survey of radio sources at 151 MHz. A 418-square-degree region centred at RA = 17h, Dec = +65deg A E Visser J M Riley H J A Roettgering E M Waldram Astron. Astrophys. Suppl. Ser. 110 419 1995 1995A&AS..110..419V radio continuum: general surveys The Cambridge Low Frequency Synthesis Telescope has been used at 151MHz to survey a region of 418 square degrees centred at RA 17^h^, Dec 65deg, which includes the North Ecliptic Cap. The resolution is 70x70''cosec {delta} and the rms noise on the maps is 25mJy beam^-1^. We present positions and flux densities for 2702 sources which have a signal to noise ratio >5.5 and radio maps of 37 selected extended sources.
7C sourcelist Name IAU name, prefixed by 7C --- RAh Beam-fitted position right ascension B1950 h RAm Beam-fitted position right ascension B1950 min RAs Beam-fitted position right ascension B1950 s DEd Beam-fitted position declination B1950 deg DEm Beam-fitted position declination B1950 arcmin DEs Beam-fitted position declination B1950 arcsec RAhC Centroid position right ascension B1950 h RAmC Centroid position right ascension B1950 min RAsC Centroid position right ascension B1950 s DEdC Centroid position declination B1950 deg DEmC Centroid position declination B1950 arcmin DEsC Centroid position declination B1950 arcsec S Beam-fitted flux density Jy Sint Integrated flux density Jy S/N Signal to noise ratio --- Extend Extent of the source in units of local beam area --- Nmax Number of local maxima within the integrated region --- Patricia Bauer CDS 1995 Jan 06 J_A+AS_110_419.xml AGN from the ROSAT all-sky survey J/A+AS/110/469 J/A+AS/110/469 AGN from the RASS AGN from the ROSAT all-sky survey N Bade H H Fink D Engels W Voges H -J Hagen L Wisotzki D Reimers Astron. Astrophys. Suppl. Ser. 110 469 1995 1995A&AS..110..469B galaxies: Seyfert quasars: general surveys X-rays: galaxies This paper presents long slit CCD spectroscopy and X-ray data of 283 AGN detected in the ROSAT-All Sky Survey (RASS). Basis of the sample is the pre-identification of 4651 RASS sources on 134 sky fields (covering in total ~3500sq.deg.). The 283 presented AGN were selected from 1253 AGN candidates resulting from the pre-identification work.
ROSAT
Optical and X-rays of the AGN No Object number --- m_No multiplicity index on object number --- Name Object name --- Code Code for used telescope number=1 Code for used telescope: (1) Calar Alto 2.2m May 1991 (2) Calar Alto 2.2m February 1992 (3) Calar Alto 2.2m May 1992 (4) Calar Alto 3.5m May 1992 (5) ESO 3.6m February 1992 (6) ESO 3.6m August 1992 (8) ESO 3.6m February 1991 (9) ESO 3.6m February 1991 (10) Calar Alto 2.2m August 1992 --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec Pos Deviation between optical and X-ray position arcsec z Redshift --- Bmag Optical magnitude B mag Count ROSAT total count rate (0.1-2.4keV) as given by the SASS ct/s e_Count rms uncertainty on count rate ct/s SX Unabsorbed X-ray flux in the total ROSAT band (0.1-2.4keV) fW/m2 e_SX rms uncertainty on X-ray flux fW/m2 XClass X-ray class as defined in Section 5 of the article --- Index energy index for the AGN of X-ray class I-III --- e_XClass rms uncertainty on X-ray class --- X-ray and line properties of the AGN No Object number --- Name Object name --- log(fX/fB) log(fX/fB) = 5.37 + log(fX) + B/2.5 --- MB Absolute optical magnitude MB mag log(Xlum) X-ray luminosity 10-7W log(NH) Galactic Hydrogen column density cm-2 EWAlpha HAlpha equivalent width 0.1nm FWHMAlpha FWHM HAlpha km/s u_FWHMAlpha Uncertainty flag on FWHMAlpha --- EWBeta HBeta equivalent width 0.1nm FWHMBeta FWHM HBeta km/s u_FWHMBeta Uncertainty flag on FWHMBeta --- l_EWDelta Limit flag on EWDelta --- EWDelta HDelta equivalent width 0.1nm FWHMDelta FWHM HDelta km/s EWMgII MgII equivalent width 0.1nm FWHMMgII FWHM for MgII km/s u_FWHMMgII Uncertainty flag on FWHMMgII --- EW[OIII]5007 Equivalent width of [OIII]5007 0.1nm [OIII]/5007 Intensity ratio [OIII]/5007 --- Additional line properties for some of the AGN No Object number --- Name Object name --- l_EWFeII1 Limit flag on EWFeII1 --- EWFeII1 FeII (blend 4500-4680) equivalent width 0.1nm u_EWFeII1 Uncertainty flag on EWFeII1 --- l_EWFeII2 Limit flag on EWFeII2 --- EWFeII2 FeII (blend 5100-5500) equivalent width 0.1nm u_EWFeII2 Uncertainty flag on EWFeII2 --- l_EW[NeV] Limit flag on EW[NeV] --- EW[NeV] Equivalent width of [NeV]3426 0.1nm l_EW[OII] Limit flag on EW[OII] --- EW[OII] Equivalent width of [OII]3727 0.1nm l_R[OII] Limit flag on R[OII] --- R[OII] Intensity ratio of [OII]3727/[OII]5007 --- l_EW[NeIII] Limit flag on EW[NeIII] --- EW[NeIII] Equivalent width of [NeIII]3869 0.1nm l_EWHGamma Limit flag on EWHGamma --- EWHGamma HGamma (possible blend with [OIII]4360) equivalent width 0.1nm l_EW[FeVII] Limit flag on EW[FeVII] --- EW[FeVII] Equivalent width of [FeVII]6087 0.1nm l_EW[FeX] Limit flag on EW[FeX] --- EW[FeX] Equivalent width of [FeX]6374 0.1nm l_EW[SII] Limit flag on EW[SII] --- EW[SII] Equivalent width of [SII]6720 0.1nm l_[SII]/Ha Limit flag on [SII]/Ha --- [SII]/Ha Intensity ratio [SII]6720/HAlpha --- Patricia Bauer CDS 1995 Feb 16 J_A+AS_110_469.xml A study of clusters and field stars in two regions in the Large Magellanic Cloud. I. CCD photometry in B and V. J/A+AS/110/533 J/A+AS/110/533 Clusters and field stars in LMC. I. A study of clusters and field stars in two regions in the Large Magellanic Cloud. I. CCD photometry in B and V. P Linde G Lynga B E Westerlund Astron. Astrophys. Suppl. Ser. 110 533 1995 1995A&AS..110..533L catalogs galaxies: stellar content Magellanic Clouds We present CCD photometry in the Johnson BV system to about V=23^m^ for the stars in six clusters and the surrounding fields in two regions of different nature in the Large Magellanic Cloud. The analysis includes estimations of loss of measured stars due to crowding effects.
*CCD B, V photometry Name Cluster name number=1 NW comp. means NW comparison area --- Id Sequence number --- X x coordinate in frame pix Y y coordinate in frame pix Vmag Johnson V mag mag B-V Johnson B-V colour index mag Patricia Bauer CDS 1994 Dec 12 J_A+AS_110_533.xml The determination of Teff of B, A and F main sequence stars from the continuum between 3200 A and 3600 A. J/A+AS/110/553 J/A+AS/110/553 Teff for B, A and F main sequence stars The determination of Teff of B, A and F main sequence stars from the continuum between 3200 A and 3600 A. N A Sokolov Astron. Astrophys. Suppl. Ser. 110 553 1995 1995A&AS..110..553S stars: atmospheres stars: early-type stars: fundamental parameters A method of determination of the effective temperature of B, A and F main sequence stars is proposed, using the slope of the continuum between 3200A and 3600A. We have determined the Balmer jump and the effective temperatures for 235 main sequence stars.
Balmer jumps, effective temperatures and their errors for the 235 program stars. HR Number in the Bright Star Catalogue --- HD Number in the Henry Draper Catalogue --- Sp Spectral Type --- E(B-V) Colour excess mag D Balmer jump (in dex) --- Teff Temperature K e_Teff rms uncertainty on temperature K Patricia Bauer CDS 1995 Jan 06 J_A+AS_110_553.xml New detections of 5_1_- 6_0_ A^+^-methanol masers towards IRAS sources J/A+AS/110/81 J/A+AS/110/81 Methanol masers towards IRAS sources New detections of 5_1_- 6_0_ A^+^-methanol masers towards IRAS sources D J van der Walt M J Gaylard G C MacLeod Astron. Astrophys. Suppl. Ser. 110 81 1995 1995A&AS..110...81V Infrared sources Masers ISM: clouds ISM: molecules masers radio lines: ISM We present the results of our second search for 6.7-GHz methanol masers towards colour-selected IRAS sources. Five hundred and twenty IRAS sources that meet the far-infrared colour criteria set by Wood & Churchwell (1989ApJ...340..265W) for ultra-compact HII regions were searched for 6.7-GHz methanol maser emission, to a sensitivity limit of 5Jy. Thirty one new maser sources were detected. We also compare the FIR colours of the newly detected maser sources with those detected by Schutte et al. (1993MNRAS.261..783S) and the IRAS counterparts of sources that have both methanol and hydroxyl maser emission. It was found that the average flux distribution of the newly detected sources differs significantly from that of all other known 6.7-GHz methanol maser sources. It is argued that the differences may be due either to intrinsic differences between the three groups of sources or to interstellar extinction. An analysis of the relation between the 6.7-GHz maser and IRAS flux densities shows that the maser flux density is always less than the 100{mu}m flux density while only three sources have a maser flux density greater than the 60{mu}m flux density. Far-infrared pumping of the 6.7-GHz methanol masers is therefore in principle viable although it was found that the apparent maser efficiency will exceed 10 per cent for a significant number of sources in the case of FIR pumping by photons between 50 and 100{mu}m. The overall detection rates on the IRAS [25-12] vs [60-12] two-colour diagram are also presented. Possible new search strategies for masers in colour-selected IRAS sources are discussed.
IRAS
Source IRAS names Note Characteristics number=1 a: Sources with no upper limits at 12, 25, 60 & 100{mu}m b: Sources with upper limit at 12 {mu}m c: Sources with upper limit at 100 {mu}m d: Sources with upper limits at 12 & 100 {mu}m --- IRAS IRAS name number=2 Misprint IRAS 06513-4316A for IRAS 16513-4316A --- Parameters of detected 6.668-GHz A^+^ -methanol masers IRAS IRAS name (Cat. <II/125>) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Vmin Velocity range (lower value) km/s Vmax Velocity range (upper value) km/s Speak Peak flux density Jy e_Speak rms uncertainty on Speak Jy Ipeak Integrated peak flux density Jy.km/s e_Ipeak rms uncertainty on Ipeak Jy.km/s James Marcout, Patricia Bauer CDS 1997 Apr 08 UNKNOWN UNKNOWN Prepared via OCR at CDS. * 31-Oct-1997: two errors in table1 detected and corrected. J_A+AS_110_81.xml On the spectral characteristics and atmospheric models of two types of white-light flares J/A+AS/110/99 J/A+AS/110/99 White-light flares models On the spectral characteristics and atmospheric models of two types of white-light flares C Fang M D Ding Astron. Astrophys. Suppl. Ser. 110 99 1995 1995A&AS..110...99F radio radiation Sun: flares X-rays: general Based on detailed analyses of the solar white-light flares (WLFs) of 1974 September 10, 1979 September 19 and 1991 October 24, the characteristics of two types of WLFs have been distinguished.
Atmospheric parameters for the non-thermal flare model, m0 = 2.5x10^-3^ Atmospheric parameters for the thermal flare model, m0 = 3.2x10^-3^ Atmospheric parameters for the pre-flare model, m0 = 2.62x10^-4^ h Heigh km m-m0 Column mass density, where m0 is the coronal mass density g/cm2 T Temperature K Vt Micro-turbulent velocity km/s N(H) Hydrogen density cm-3 Ne Electron density cm-3 table.tex LaTeX version of the tables Patricia Bauer CDS 1994 Oct 28 J_A+AS_110_99.xml Systematic search for UV-excess quasar candidates in 40 square degrees at the North Galactic Pole J/A+AS/111/169 J/A+AS/111/169 UV-excess quasar candidates Systematic search for UV-excess quasar candidates in 40 square degrees at the North Galactic Pole O Moreau H Reboul Astron. Astrophys. Suppl. Ser. 111 169 1995 1995A&AS..111..169M astrometry quasars: general stars: Population II surveys techniques: photometric white dwarfs We have developed a procedure (so called PAPA) for measurement of magnitudes (about 0.1mag accurate) and positions (with accuracy better than 0.5arcsec) of all the objects present on photographic plates digitised with the MAMA machine. This homogeneous procedure was applied to four Schmidt plates - in U, B and twice V - covering the Palomar-Sky-Survey field PS +30deg 13h00m, a 40-square-degree zone at the North Galactic Pole. A general-interest exhaustive tricolour catalogue of 19542 star-like objects down to V=20.0 has been produced and we selected 1681 quasar candidates on the basis of ultraviolet excess and, when possible, absence of any measurable proper motion. The astrometric and photometric catalogue of the candidates is given in electronic form.
UVX objects already spectroscopically identified (table 7 of paper) White-dwarf candidates (from table 8 of paper) Quasar-candidate catalogue (section 6 of paper) N Detection number --- Name Identification --- RAh Right ascension 2000 h RAm Right ascension 2000 min RAs Right ascension 2000 s DE- Declination sign --- DEd Declination 2000 deg DEm Declination 2000 arcmin DEs Declination 2000 arcsec Umag U magnitude mag u_Umag Uncertainty flag on Umag --- Bmag B magnitude mag u_Bmag Uncertainty flag on Bmag --- Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag --- Rem Remarks number=1 Symbols used in the tables: (section 6 of paper) NPM a proper motion could have been measured, if any greater than 0.07"/year BG the local sky background has been flagged (section 4.3) in U, B and/or V NBQS not in the BQS though measured with B < 16 and U-B < -0.65 QSO quasar Sy Seyfert galaxy AG active galaxy WD white dwarf sd subdwarf (sdO for a subdwarf O, ...) HBB B horizontal branch star NHB a star which may be a HB or a normal one PNN planetary nebula nucleus em. emission line object --- Patricia Bauer CDS 1995 Jan 16 J_A+AS_111_169.xml High-resolution abundance analysis of two stars near the globular cluster NGC 6522 projected in Baade's window. J/A+AS/111/17 J/A+AS/111/17 Abundance analysis of stars in NGC 6522 High-resolution abundance analysis of two stars near the globular cluster NGC 6522 projected in Baade's window. S Castro B Barbuy E Bica S Ortolani A Renzini Astron. Astrophys. Suppl. Ser. 111 17 1995 1995A&AS..111...17C stars: abundances Galaxy: halo globular clusters: general The CASPEC echelle spectrograph at the ESO 3.6 m telescope was used to obtain high resolution spectra of Arp 1145 and Arp 2240, two stars of the Baade Window, near the globular cluster NGC 6522. From a detailed analysis using equivalent widths and spectrum synthesis we derive the stellar parameters (T_eff_, log g and [M/H])=(4750,1.2,-0.9) and (5000,2.15,+0.2), respectively for Arp 1145 and Arp 2240.
Equivalent widths of Arp 1145 and Arp 2240 Lambda Wavelength 0.1nm El Element --- Ioniz Ionization stage --- ExcPot Excitation potential eV loggf Oscillator strength (log gf) --- WArp1145 Equivalent widths for Arp1145 0.1pm WArp2240 Equivalent widths for Arp2240 0.1pm Patricia Bauer CDS 1994 Dec 20 J_A+AS_111_17.xml CCD measurements of visual binaries J/A+AS/111/229 J/A+AS/111/229 CCD meas. of visual binaries CCD measurements of visual binaries C Abad F Della Prugna Astron. Astrophys. Suppl. Ser. 111 229 1995 1995A&AS..111..229A astrometry binaries: visual We report CCD measurements of 33 visual double stars observed at the 1-meter coude reflector of the Observatorio de Llano del Hato located at Merida, Venezuela. We also present an algorithm to determine the stars' centroids for superimposed images as well as a brief comparison of accuracies attained by the algorithm and the program CENTER of the IRAF package.
CCD measurements Average A '*' indicates that the following data are averaged values --- Name ADS number or name of the pair --- RAh Right Ascension J2000.0 h RAm Right Ascension J2000.0 min DE- Declination sign --- DEd Declination J2000.0 deg DEm Declination J2000.0 arcmin Vmin Magnitude of the components(minimal value) mag n_Vmin Separator - --- Vmax Magnitude of the components (maximal value) mag Date Epoch of observation yr rho Angular separation arcsec e_rho rms uncertainty on rho arcsec o_rho Number of images contributing to the separation result --- PA Position angle deg e_PA rms uncertainty on PA deg o_PA Number of images contributing to the position angle result --- Patricia Bauer CDS 1995 Jan 13 J_A+AS_111_229.xml Mainline OH detection rates from blue circumstellar shells J/A+AS/111/237 J/A+AS/111/237 OH detections from circumstellar shells Mainline OH detection rates from blue circumstellar shells B M Lewis P David A M Le Squeren Astron. Astrophys. Suppl. Ser. 111 237 1995 1995A&AS..111..237L V/68 : catalog of observations for stellar masers (Benson+ 1990) Masers Stars, radio circumstellar matter masers radio lines: stars stars: AGB and post-AGB We identified 240 accessible circumstellar shells with water and/or SiO masers, and used the Arecibo and Nancay radio telescopes to search for mainline OH emission from them. Our targets are often Mira variables without previously known mainline masers. This search results in 89 detections, of which 77 are new.
Target list for mainline search IRAS IRAS (cat. <II/125>) name --- Name Alternative name --- Vel Central search velocity km/s r_Vel Reference for velocity number=1 Velocity References: A Arcetri list: Cesaroni et al A&AS 76, 445 (=1988A&AS...76..445C) B Benson et al. ApJS,74, 911 (=1990ApJS...74..911B) E Effelsberg unpublished water (Lewis and Engels) H Haystack unpublished water (Lewis 1995) Hk Haikala A&A, 85, 875 P1 Allen et al., MN 236, 363 (=1989MNRAS.236..363A) P2 Hall et al., MN 243, 480 (=1990MNRAS.243..480H) P3 Hall et al., MN 247, 549 (=1990MNRAS.247..549H) CO Margulis et al., ApJ,361, 673 (=1990ApJ...361..673M) --- Mainline Mainline status number=2 D = detected; N = not detected Mainline status other than those originating here: s: Sivagnanam et al. A&A, 206, 285 (=1988A&A...206..285S) b: Benson et al. ApJS,74, 911 (=1990ApJS...74..911B) *: Norris et al., Aust.Astr.J, 5, 662 n: other papers from Nancay a: other papers from Arecibo --- Water Water status number=2 D = detected; N = not detected Mainline status other than those originating here: s: Sivagnanam et al. A&A, 206, 285 (=1988A&A...206..285S) b: Benson et al. ApJS,74, 911 (=1990ApJS...74..911B) *: Norris et al., Aust.Astr.J, 5, 662 n: other papers from Nancay a: other papers from Arecibo --- SiO SiO status number=2 D = detected; N = not detected Mainline status other than those originating here: s: Sivagnanam et al. A&A, 206, 285 (=1988A&A...206..285S) b: Benson et al. ApJS,74, 911 (=1990ApJS...74..911B) *: Norris et al., Aust.Astr.J, 5, 662 n: other papers from Nancay a: other papers from Arecibo --- OH OH status (mainline plus 1612 MHz) number=2 D = detected; N = not detected Mainline status other than those originating here: s: Sivagnanam et al. A&A, 206, 285 (=1988A&A...206..285S) b: Benson et al. ApJS,74, 911 (=1990ApJS...74..911B) *: Norris et al., Aust.Astr.J, 5, 662 n: other papers from Nancay a: other papers from Arecibo --- Observer Observer --- 25-12 (25-12) colour number=3 (25-12) = log10(S(25)*12*0.89 / S(12)*25*1.09) where S(25) is the flux at 25um and S(12) is the flux at 12um --- 60-25 (60-25) colour number=4 (60-25) = log10(S(60)*25*0.82 / S(25)*60*0.89) where S(60) is the flux at 60um and S(25) is the flux at 25um --- Mainline data for detections IRAS IRAS name --- V1667l 1667MHz low velocity peak km/s V1667h 1667MHz high velocity peak km/s V1665l 1665MHz low velocity peak km/s V1665h 1665MHz high velocity peak km/s I1667l 1667MHz low peak intensity mJy I1667h 1667MHz high peak intensity mJy I1665l 1665MHz low peak intensity mJy I1665h 1665MHz high peak intensity mJy Sint1667 integrated 1667 flux mJy.km/s Sint1665 integrated 1665 flux mJy.km/s Full sample of objects with water or SiO masers IRAS IRAS name --- Mainline Mainline status number=1 D=detected, N=not detected, 0=not available --- OH OH status (main and/or 1612MHz) --- 25-12 (25-12) IR colour number=2 (25-12) = log10(S(25)*12*0.89 / S(12)*25*1.09) where S(25) is the flux at 25um and S(12) is the flux at 12um --- 60-25 (60-25) IR colour number=3 (60-25) = log10(S(60)*25*0.82 / S(25)*60*0.89) where S(60) is the flux at 60um and S(25) is the flux at 25um --- GLAT Galactic latitude deg GLON Galactic longitude deg S25 IRAS (cat. <II/125>) 25 micron flux Jy Sp LRS spectral class --- Water Water status number=1 D=detected, N=not detected, 0=not available --- SiO SiO status number=1 D=detected, N=not detected, 0=not available --- Patricia Bauer CDS 1995 Jan 12 J_A+AS_111_237.xml A catalogue of velocities in the central regions of the Coma cluster J/A+AS/111/265 J/A+AS/111/265 Velocities in Coma cluster A catalogue of velocities in the central regions of the Coma cluster A Biviano F Durret D Gerbal O Le Fevre C Lobo A Mazure E Slezak Astron. Astrophys. Suppl. Ser. 111 265 1995 1995A&AS..111..265B VII/42A : GMP Catalogue by Godwin J.G., Metcalfe N. and Peach J.V. =1983MNRAS.202..113G VII/99 : Catalogue of Radial Velocities of Galaxies by Palumbo G.G.C., Tanzella-Nitti G., Vettolani G. galaxies: clusters: individual (Coma cluster) galaxies: distances and redshifts We present a catalogue of velocities for 305 objects in a field of 48x25arcmin^2^, centered between the galaxies NGC 4889 and NGC 4874, as well as in a field of 10x10arcmin^2^ centered on NGC 4839, in the Coma cluster. Of these velocities, 225 are new measurements, 78 of which for objects with at least one velocity already available in the literature before our survey. Our sample is 95% complete in redshift up to a magnitude b_26.5_=18.0.
Central region of Coma Cluster A 10x10' region around NGC 4389 n_GMP The asterisk indicates that the number corresponds to the unpublished star catalogue of the same GMP authors; --- GMP Number in the catalogue of Godwin, Metcalfe & Peach <VII/42A> --- OtherName Other (NGC or IC) designation --- Xpos Position westwards from cluster center number=1 the position of the cluster center is: 12 57.3 +28 14.4 (1950) arcsec Ypos Position northwards from cluster center number=1 the position of the cluster center is: 12 57.3 +28 14.4 (1950) arcsec b26.5 Blue magnitude at 26.5 mag/arcsec2 isophote (from GMP) mag b-r colour from GMP catalogue mag cz Heliocentric velocity km/s e_cz error on cz when available; for our data, errors from the RVSAO package in IRAF. km/s r_cz Reference to the velocity number=2 References are: 1: this paper 2: Caldwell N., Rose J.A., Sharples R.M., Ellis R.S., Bower R.G. =1993AJ....106..473C 3: Mazure A., Proust D., Mathez G., Mellier Y. =1988A&AS...76..339M 4: Palumbo G.G.C., Tanzella-Nitti G., Vettolani G., 1983, "Catalogue of Radial Velocities of Galaxies", Gordon & Breach Science Publishers, Paris <VII/99> --- q_cz quality class of our redshifts, from 1 (best) to 3; --- n_cz 'E' indicates presence of emission lines in our spectra. --- Francois Ochsenbein CDS 1995 Oct 05 Andrea Biviano <biviano@strw.leidenuniv.nl> J_A+AS_111_265.xml BV(RI)KC CCD photometry of the core of the young open cluster, NGC 5460 J/A+AS/111/275 J/A+AS/111/275 BVRI CCD photometry of NGC 5460 BV(RI)KC CCD photometry of the core of the young open cluster, NGC 5460 D Barrado P B Byrne Astron. Astrophys. Suppl. Ser. 111 275 1995 1995A&AS..111..275B Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 5460) We present CCD photometry on the BV(RI)_KC_ (Cape) photometric system of the core of the young open cluster, NGC 5460, to a magnitude limit V=~19, R=~19.5. We give photometry for 353 stars and identify 25 as cluster members along with a further 27 as possible members based on their positions in individual colour-magnitude diagrams. We estimate the reddening to the cluster and redefine its distance and age. Four stars are identified as possible variables and their nature discussed.
Positions, BV(RI) photometry and membership status of stars in the field of NGC 5460 No Star number --- RAh Right ascension 1984.5 (See Historical Notes) h RAm Right ascension 1984.5 min RAs Right ascension 1984.5 s DE- Declination sign --- DEd Declination 1984.5 deg DEm Declination 1984.5 arcmin DEs Declination 1984.5 arcsec Bmag B magnitude mag Vmag V magnitude mag Rmag R magnitude mag Imag I magnitude mag Memb Membership status number=1 M: member; PM: possible member; NM: non-member --- Name Other identifications number=2 Equivalent name according to Claria J.J., Lapasset E., Bosio M.A., 1993, A&AS, 99, 1 --- table2.tex LaTeX Version of Table 2 Patricia Bauer CDS 1995 Jul 17 UNKNOWN UNKNOWN * 21-Feb-1995: table prepared at CDS from data provided by the authors * 17-Jul-1995: the equinox indicated in the "Bytye-by-byte description" was corrected from the erroneous value 1950 into 1984.5, after contacting the authors <pbb@star.arm.ac.uk> and <dbn@astro2.fis.ucm.es> J_A+AS_111_275.xml A radio continuum study of the Magellanic Clouds. Part IV: Catalogues of radio sources in the Large Magellanic Cloud at 1.40, 2.45, 4.75, 4.85 and 8.55 GHz J/A+AS/111/311 J/A+AS/111/311 Radio continuum study of the MC A radio continuum study of the Magellanic Clouds. Part IV: Catalogues of radio sources in the Large Magellanic Cloud at 1.40, 2.45, 4.75, 4.85 and 8.55 GHz M D Filipovic R F Haynes G L White P A Jones U Klein R Wielebinski Astron. Astrophys. Suppl. Ser. 111 311 1995 1995A&AS..111..311F VIII/38 : The PMN (Parkes-MIT-NRAO) Catalogue J/A+AS/121/321 : SMC catalogue of radiosources (Filipovic+ 1997) Clarke J.N. et al. 1976 Aust. J. Phys. Astrophys. Suppl. 40, 1 (1976AuJPS..40....1C) Cohen R. et al. 1988 ApJ 331, L95 (1988ApJ...331L..95C) Davies R.D. et al. 1976 Mem. R. Astr. Soc. 81, 89 (1976MmRAS..81...89D) Henize K.G. 1956 ApJS 2,315 (1955ApJS....2..315H) Long K.S. et al. 1981 ApJ 248, 925 (1981ApJ...248..925L) Lucke P.B. et Hodge P.W. 1970 AJ 75, 171 (1970AJ.....75..171L) McGee R.X. et al. 1972a Aust. J. Phys. 25, 613 (1972AuJPh..25..613M) McGee R.X. et al. 1972b Aust. J. Phys. 25, 581 (1972AuJPh..25..581M) Sanduleak N. et al. 1978 PASP 90, 621 (1978PASP...90..621S) Sanduleak N. 1984 eds. S. Van de Bergh, K.S. de Boer, Proc. IAU Symp. 108, Structure and evolution of the Magellanic Clouds (Reidel, Dordrecht) 231 (1984IAUS..108..231S) Sinnot R.W. NGC 2000 1988 (Cambridge University Press) 46, cat. <VII/118> Taylor J.H. et al. 1993 ApJS 88,529 (1993ApJS...88..529T) Wang Q. et al. 1981 ApJ 374, 475 (1991ApJ...374..475W) Wright A.E. et al. 1994 ApJS 91, 111 (1994ApJS...91..111W) Magellanic Clouds Radio sources catalogs galaxies: individual (LGM) radio continuum: galaxies radio continuum: general From observations with the Parkes radio telescope, we present catalogues of radio sources in the Large Magellanic Cloud at four frequencies: 1.40, 2.45, 4.75 and 8.55GHz, and an additional catalogue from a source analysis of the Parkes-MIT-NRAO survey at 4.85GHz. A total of 469 sources have been detected at least one of these frequencies, 132 of which are reported here for the first time as radio sources.
Catalogue of LMC sources at 1.40 GHz Catalogue of LMC sources at 2.45 GHz Catalogue of LMC sources at 4.75 GHz Catalogue of LMC sources at 4.85 GHz Catalogue of LMC sources at 8.55 GHz Source Source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin Des Declination (1950) arcsec SType Source type: when 'e' source is significantly extended --- FDens Flux density Jy Source cross-reference Number Source number --- Source Source name --- Comments Other names and comments number=1 The following acronyms are used: N Henize (1955ApJS....2..315H) MC McGee et al (1972AuJPh..25..581M, 1972AuJPh..25..613M) MC4 Clarke et al. (1976AuJPS..40....1C) DEM Davies et al. (1976MmRAS..81...89D) LHG Long et al. (1981ApJ...248..925L) W Wang et al. (1991ApJ...374..475W) NGC Sinnot (1988, cat. <VII/118>) PMN Wright et al. (1994ApJS...91..111W) PSR Taylor et al. (1993ApJS...88..529T) LH Lucke et Hodge (1970AJ.....75..171L) Sa Sanduleak et al. (1978PASP...90..621S) and Sanduleak (1984IAUS..108..231S) CO Cohen et al. (1988ApJ...331L..95C) --- Simona Mei CDS 1995 Jun 07 J_A+AS_111_311.xml Study of variability of the polarization in Herbig Ae/Be stars J/A+AS/111/399 J/A+AS/111/399 Polarization variability in Herbig Ae/Be stars Study of variability of the polarization in Herbig Ae/Be stars S K Jain H C Bhatt Astron. Astrophys. Suppl. Ser. 111 399 1995 1995A&AS..111..399J polarization stars: emission-line, Ae stars: pre-main sequence stars: variables: general We report our measurements of linear polarization of a number of Herbig Ae/Be stars made at several epochs during the period 1989-1993. These results together with the observations compiled from the published sources have been analysed to study the variability of polarization in Herbig Ae/Be stars. It is found that polarimetric variability is a common feature of this class of objects. Most of the objects are variable on time scales >=1yr. Some objects have shown large variations on time scales as short as ~1 month indicating structural changes in the distribution of circumstellar matter close to the star within a few tens of stellar radii. Variations in the polarization position angle are not always correlated with variations in the degree of polarization.
Polarimetric data for Herbig Ae/Be stars SN Sequential number --- Name Object name ---- Date observation date --- pU Degree of polarization in U filter % e_pU rms uncertainty on pU % paU Position angle in U filter deg e_paU rms uncertainty on paU deg pB Degree of polarization in B filter % e_pB rms uncertainty on pB % paB Position angle in B filter deg e_paB rms uncertainty on paB deg pV Degree of polarization in V filter % e_pV rms uncertainty on pV % paV Position angle in V filter deg e_paV rms uncertainty on paV deg pR Degree of polarization in R filter % e_pR rms uncertainty on pR % paR Position angle in R filter deg e_paR rms uncertainty on paR deg pI Degree of polarization in I filter % e_pI rms uncertainty on pI % paI Position angle in I filter deg e_paI rms uncertainty on paI deg ref References number=1 References: 1 Present work 2 Garrison M. Jr, Anderson C.M. 1978, 221, 601 Bull. Astron.Soc.India, 21, 541 3 Jain S.K., Bhatt H.C., Ram Sagar, 1990, A&AS, 83, 237 4 Vbra F.J. 1975, ApJ, 195, 101 5 Vrba F.J. Schmidt G.D., Hintzen P.M. 1979, ApJ, 227, 185 --- table1.tex TeX version of table1 Patricia Bauer CDS 1994 Nov 21 J_A+AS_111_399.xml Red and reddened stars in the region of Cygnus OB2 (VI Cygni) association. J/A+AS/111/407 J/A+AS/111/407 VI Cygni red & reddened stars Red and reddened stars in the region of Cygnus OB2 (VI Cygni) association. M Parthasarathy S K Jain Astron. Astrophys. Suppl. Ser. 111 407 1995 1995A&AS..111..407P galaxies: individual (Sculptor) galaxies: stellar content Hertzsprung-Russell (HR diagram) Local Group stars: horizontal-branch stars: variables: other From an ultra-low dispersion spectroscopic survey of the Cyg OB2 association several red and reddened stars are detected. Most of these stars appear to be reddened early-type stars belonging to the Cygnus OB2 association. The distance moduli V_0_-M_v_=11.2 and minimum reddening E(B-V)=1.2 suggests that some of the red stars in the magnitude range 15 to 17 are most likely reddened late B and early A main sequence stars of the Cyg OB2 association.
Red and reddened stars in the region of Cygnus OB2 (VI Cygni) association SeqNunb Sequential number --- Ref1 Number of the star in Reddish et al. (1967). The number in parenthesis gives the field number in Reddish et al. (1967). NI indicates new identification --- Vmag Visual magnitude mag B-V B-V colour mag Grid Grid identification (Fig. No/grid) --- Ref2 Number of the star in Massey &Thompson (1991) --- Patricia Bauer CDS 1995 Feb 17 J_A+AS_111_407.xml CCD photometry of 11 resolved dwarf irregular galaxies J/A+AS/111/527 J/A+AS/111/527 CCD photometry of 11 dwarf irregular galaxies CCD photometry of 11 resolved dwarf irregular galaxies U Hopp R E Schulte-Ladbeck Astron. Astrophys. Suppl. Ser. 111 527 1995 1995A&AS..111..527H galaxies: irregular galaxies: stellar content We present CCD imaging and photometry in B and Cousins R of the dwarf irregular galaxies UGC 4459 (=DDO 53), UGC 5272 (A=DDO 64 and B), UGC 5340 (=DDO 68), UGC 6456, UGC 7559 (=DDO 126), UGC 8024 (=NGC 4789A=DDO 154), UGC 8091 (= GR 8=DDO 155), UGC 8320 (=DDO 168), UGC 8760 (=DDO 183), and DDO 210. For DDO 210 we also give results in the V filter. Photometry of the resolved stars was carried out on background-subtracted images using DAOPHOT. The tables of measurements include positions, magnitudes, colors, a magnitude error, and a color error. Integrated fluxes and colors are also reported. The single-star photometry is compared to previous results in three of the galaxies (UGC 8024, UGC 8091, DDO 210).
BR photometry of resolved sources in UGC 4459 BR photometry of resolved sources in UGC 7759 BR photometry of resolved sources in UGC 8024 BR photometry of resolved sources in UGC 8091 BR photometry of resolved sources in UGC 5272 A and B BR photometry of resolved sources in UGC 5340 BR photometry of resolved sources in UGC 6456 BR photometry of resolved sources in UGC 8320 BR photometry of resolved sources in UGC 8760 ID Running number --- Xpos Relative x frame coordinate arcsec Ypos Relative y frame coordinate arcsec Bmag B magnitude of object mag B-R B-R colour index mag e_Bmag rms uncertainty on Bmag mag e_B-R rms uncertainty on B-R mag BV photometry of resolved sources in DDO 210 ID Running number --- Xpos Relative x frame coordinate arcsec Ypos Relative y frame coordinate arcsec Vmag V magnitude of object mag B-V B-V colour index mag e_Vmag rms uncertainty on Vmag mag e_B-V rms uncertainty on B-V mag VR photometry of resolved sources in DDO 210 ID Running number --- Xpos Relative x frame coordinate arcsec Ypos Relative y frame coordinate arcsec Vmag V magnitude of object mag V-R V-R colour index mag e_Vmag rms uncertainty on Vmag mag e_V-R rms uncertainty on V-R mag Patricia Bauer CDS 1995 Feb 13 J_A+AS_111_527.xml Synthetic absorption line strengths in star forming regions, and the effects on the helium abundance determination J/A+AS/111/57 J/A+AS/111/57 Synthetic absorption in star forming regions Synthetic absorption line strengths in star forming regions, and the effects on the helium abundance determination K Olofsson Astron. Astrophys. Suppl. Ser. 111 57 1995 1995A&AS..111...57O galaxies: evolution galaxies: stellar content HII regions line: profiles stars: luminosity function, mass function Spectral evolutionary calculations have been employed in order to follow the behaviour of absorption lines in single-burst star forming regions. The model calculations are based on theoretical evolutionary tracks and model atmosphere stellar spectra at 5A resolution and they include the pre-main sequence phase. Three different metallicities have been considered; Z=0.001, 0.008 and 0.020, this range covers easily the one occupied by blue compact dwarf galaxies. This analysis focuses on the post-active burst phase and follows the evolution up to 15 million years after the episode of star formation has ceased, using an instantaneous burst of star formation. The absorption lines included are hydrogen, neutral and once ionized helium. Non-LTE absorption line profiles have been implemented to these lines, also at a 5A resolution. The equivalent widths and line profiles are studied as a function of lower and upper mass limits and slope of the mass function as well as the age. It is shown that the equivalent widths of the Balmer lines are increasing during the course of evolution, while the strength of the neutral and ionized helium lines decreases monotonically. Both the hydrogen and helium lines show high sensitivity to variations in the initial mass function (IMF). The Balmer line equivalent widths range from about 1.5 to 6.5A, depending on the IMF parameters used. As anticipated, these numbers are rather insensitive to the metallicity. Contrary to what has been claimed, the Balmer lines are prominent even if the lower mass limit is as high as 10M_{sun}_. It has been proposed that the weak hydrogen lines sometimes seen in starburst galaxies, often interpreted as evidence for a deficiency in low mass stars, could be due to the finite lifetimes of pre-main sequence stars. This analysis shows that it is very much dependent on the slope of the mass function. The equivalent width of the HeI-4471A line never exceeds 0.35A for any choice of the IMF parameters while the equivalent width of the HeII-4686A line reaches at the most 0.20A using the most top-heavy IMF. As expected, these numbers are only slightly dependent on the metallicity in the optical spectral region.
Line fluxes for hydrogen lines Line fluxes for neutral helium lines Line fluxes for once ionized helium lines Z Metallicity --- Mod Model number --- Line Line considered --- dl Continuum number=1 The wavelength-range is 40A on either side of the centre of the line dl and normalized to 1.000 on the leftmost wavelength point at the age of 1 Myr 0.1nm F1Myr Line flux for Age=1Myr number=2 The fluxes are presented with a resolution of 5A 0.1nm F2Myr Line flux for Age=2Myr number=2 The fluxes are presented with a resolution of 5A 0.1nm F4Myr Line flux for Age=4Myr number=2 The fluxes are presented with a resolution of 5A 0.1nm F6Myr Line flux for Age=6Myr number=2 The fluxes are presented with a resolution of 5A 0.1nm F8Myr Line flux for Age=8Myr number=2 The fluxes are presented with a resolution of 5A 0.1nm F10Myr Line flux for Age=10Myr number=2 The fluxes are presented with a resolution of 5A 0.1nm F15Myr Line flux for Age=15Myr number=2 The fluxes are presented with a resolution of 5A 0.1nm Patricia Bauer CDS 1995 Jan 16 J_A+AS_111_57.xml A deep UBVRI CCD photometric study of the moderately young southern open star cluster NGC 4755 = {kappa} Crucis J/A+AS/111/75 J/A+AS/111/75 UBVRI CCD photometry of NGC 4755 A deep UBVRI CCD photometric study of the moderately young southern open star cluster NGC 4755 = {kappa} Crucis R Sagar R D Cannon Astron. Astrophys. Suppl. Ser. 111 75 1995 1995A&AS..111...75S Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 4755) stars: formation CCD observations in U, B, V, R and I passbands have been used to generate (U-B), (B-V) colour-colour and deep V, (B-V); V, (U-B) and V, (V-I) colour-magnitude diagrams for the young open cluster NGC 4755. The sample consists of 813 stars reaching down to V about 20mag.
UBVRI photometry Region Region number number=1 The center of Region 1 is located ~3.2 arcmin south-west while that of Region 2 ~3.5 arcmin north-east to the cluster center marked by Dachs & Kaiser (1984). --- No star number --- X X coordinate pix Y Y coordinate pix Vmag V magnitude mag U-B U-B colour mag B-V B-V colour mag V-R V-R colour mag V-I V-I colour mag o_Umag Number of observations in U --- o_Bmag Number of observations in B --- o_Vmag Number of observations in V --- o_Rmag Number of observations in R --- o_Imag Number of observations in I --- OtherName Cross identification of stars. number=2 Stars observed by Arp & van Sant (1958) and Dachs & Kaiser (1984) in the photoelectric and photographic system have been prefixed with AV and DK respectively. The candidates for pre-main sequence stars are identified as PMS in the last column. --- Patricia Bauer CDS 1995 Jan 06 J_A+AS_111_75.xml A detailed study of the open cluster Pismis 20 J/A+AS/111/85 J/A+AS/111/85 Open cluster Pis 20 A detailed study of the open cluster Pismis 20 R A Vazquez J -M Will P Prado A Feinstein Astron. Astrophys. Suppl. Ser. 111 85 1995 1995A&AS..111...85V open clusters and associations: individual (Pis 20) stars: individual (WR 67) stars: luminosity function, mass function stars: Wolf-Rayet white dwarfs The very young open cluster Pis 20 has been investigated using CCD UBVR photometry. New blue faint members were found down to V=19mag. With them we obtain a better definition of the lower cluster main sequence. Using the fitting method, we derive a cluster distance of d=3600pc (V_0_-M_V_=12.80). The mean color excess is <E_B-V_>=1.24mag.
Observed colors and magnitudes in Pismis 20 SeqNum Sequential star number --- X X position --- Y Y position --- Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag number=1 ' :' indicates stars with error from 0.07 to 0.10 mag '::' indicates stars with errors larger than 0.10 mag --- B-V B-V colour index mag u_B-V Uncertainty flag on B-V number=1 ' :' indicates stars with error from 0.07 to 0.10 mag '::' indicates stars with errors larger than 0.10 mag --- U-B U-B colour index mag u_U-B Uncertainty flag on U-B number=1 ' :' indicates stars with error from 0.07 to 0.10 mag '::' indicates stars with errors larger than 0.10 mag --- V-R V-R colour index mag u_V-R Uncertainty flag on V-R number=1 ' :' indicates stars with error from 0.07 to 0.10 mag '::' indicates stars with errors larger than 0.10 mag --- Intrinsic colors, magnitudes and masses of Pismis 20 stars SeqNum Sequential star number --- V0 Intrinsic V magnitude mag (B-V)0 Intrinsic B-V colour index mag E(B-V) B-V colour excess mag (U-B)0 Intrinsic U-B colour index mag E(U-B) U-B colour excess mag MV Absolute V magnitude mag Mass Star mass solMass Rem Remarks number=1 (a) indicates that color excesses were computed through a relation between spectral types and color indices following Schmidt-Kaler (1982 in: Landolt-Bornstein, Neue Serie VI/2b) (b) V_0_ was obtained adopting a mean cluster reddening <E_B-V_ >= 1.24. The mass corresponds to the most massive cluster star (*) denotes possible members --- Patricia Bauer CDS 1995 Jan 16 J_A+AS_111_85.xml Studies of dense molecular cores in regions of massive star formation II. CSJ=2-1 survey of southern H_2_O masers in the longitude range l=260deg-310deg. J/A+AS/111/95 J/A+AS/111/95 Studies of dense molecular cores Studies of dense molecular cores in regions of massive star formation II. CSJ=2-1 survey of southern H_2_O masers in the longitude range l=260deg-310deg. I Zinchenko K Mattila M Toriseva Astron. Astrophys. Suppl. Ser. 111 95 1995 1995A&AS..111...95Z ISM: clouds ISM: molecules masers radio lines: ISM stars: formation We searched for the CS J=2-1 emission towards 30 southern H_2O and OH masers with the SEST radio telescope (29 H_2O and H_2O/OH masers and 1 OH maser). We detected and mapped 24 CS emitting regions associated probably with 27 H_2O masers. The C^34^S J=2-1 and CO J=1-0 lines were also observed at the grid positions closest to the CS peaks. Here we present the CS maps and the spectra at the peak positions along with the CO and C^34^S spectra. We derive the C^34^S column densities in the LTE approximation and discuss briefly the spatial and kinematic structure of the sources. The association with the IRAS point sources and small scale structure sources is examined. We estimate the kinematic distances to the cores and derive their sizes, masses and mean densities. The velocity differences between the masers and CS cores are analyzed. The CO and CS spectra towards several sources demonstrate deep absorption features. We argue that they can be due to extended low excitation foreground cloud(s).
Sources Name Name of the source --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec DTheta Uncertainty on coordinates arcmin R Galacto-centric distance kpc Z1 Lowest value of height above the galactic plane when n_Z='/' pc n_Z '/' indicates an interval of Z --- Z Z or higher value of Z when n_Z='/' pc Dist1 Lowest value of kinematic distances when n_Dist='/' kpc n_Dist '/' indicates an interval of Dist --- Dist Kinematic distance or the highest value of kinematic distance when n_Dist='/' kpc Dstar1 Spectrophotometric distance of the exciting star (first detection) kpc r_Dstar1 Reference for Dstar1 number=1 a) Brand J. & Blitz L., 1993, A&A 275, 67 b) Avedisova V.S. & Palous J., 1989, Bull. Astron. Inst. Czechosl. 40, 42 c) Georgelin Y.M. & Geogerlin Y.P., 1976, A&A 49, 57. --- Dstar2 Spectrophotometric distance of the exciting star (second detection) kpc r_Dstar2 Reference for Dstar2 number=1 a) Brand J. & Blitz L., 1993, A&A 275, 67 b) Avedisova V.S. & Palous J., 1989, Bull. Astron. Inst. Czechosl. 40, 42 c) Georgelin Y.M. & Geogerlin Y.P., 1976, A&A 49, 57. --- Dstar3 Spectrophotometric distance of the exciting star (third detection) kpc r_Dstar3 Reference for Dstar3 number=1 a) Brand J. & Blitz L., 1993, A&A 275, 67 b) Avedisova V.S. & Palous J., 1989, Bull. Astron. Inst. Czechosl. 40, 42 c) Georgelin Y.M. & Geogerlin Y.P., 1976, A&A 49, 57. --- VH2Oinf Lowest value of radial velocity of the maser when n_VH2O=',' km/s n_VH2O ',' indicates an interval of values --- VH2O Radial velocity of the maser or highest value of VH2O when n_VH2O=',' km/s Rem Remarks --- Line areas and gaussian line parameters Source Name of the source --- Dalpha Delta right ascension min DDE Delta declination arcmin Int(Tmb)1 Integral of the main beam brightness temperature in dv (Line areas) (CS) K.km/s e_Int(Tmb)1 Statistical uncertainties on Line areas (CS) 0.1K.km/s Tmb1 Main beam brightness temperature (CS) K e_Tmb1 Statistical uncertainties on main beam brightness temperature (CS) 0.01K Vel1 LSR velocity (CS) km/s e_Vel1 Statistical uncertainties on velocity (CS) 0.01km/s DVel1 Delta velocity (CS) km/s e_DVel1 Statistical uncertainties (CS) 0.01km/s Int(Tmb)2 Integral of the main beam brightness temperature in dv (Line areas)(C^34^S) K.km/s e_Int(Tmb)2 Statistical uncertainties on Line areas (C^34^S) 0.01K.km/s Tmb2 Main beam brightness temperature (C^34^S) K e_Tmb2 Statistical uncertainties on main beam brightness temperature (C^34^S) 0.01K Vel2 Velocity (C^34^S) km/s e_Vel2 Statistical uncertainties on velocity (C^34^S) 0.01km/s DVel2 Delta velocity (C^34^S) km/s e_DVel2 Statistical uncertainties (C^34^S) 0.1km/s Tmb3 Main beam brightness temperature (CO) K n_Tmb3 Label on the main beam brightness temperature (CO) that indicates position (0,0) --- Sources associated Name Source name --- IRAS IRAS name --- RAs Right ascension (seconds) s DEm Declination (arcmin) arcmin DEs Declination (arcsec) arcsec F12 Flux at 12um for IRAS point sources Jy q_F12 Flux quality flags for F12 number=1 The flux quality flags are shown following the notation in the IRAS point source and small scale structure catalogues --- F25 Flux at 25um for IRAS point sources Jy q_F25 Flux quality flags for F25 number=1 The flux quality flags are shown following the notation in the IRAS point source and small scale structure catalogues --- F60 Flux at 60um for IRAS point sources Jy q_F60 Flux quality flags for F60 number=1 The flux quality flags are shown following the notation in the IRAS point source and small scale structure catalogues --- F100 Flux at 100um for IRAS point sources Jy q_F100 Flux quality flags for F100 number=1 The flux quality flags are shown following the notation in the IRAS point source and small scale structure catalogues --- Column densities, sizes, mean densities, masses Source Source name --- logNl Column density of the core (C34S) cm-2 e_logNl Rms uncertainty on column density 0.01cm-2 L Size of the core pc logn Mean density of the core cm-3 M Mass of the core solMass Patricia Bauer CDS 1995 Mar 02 J_A+AS_111_95.xml Dust around young stars. Photopolarimetric observations of the T Tauri star BM Andromedae J/A+AS/112/457 J/A+AS/112/457 Photopolarimetry of BM And Dust around young stars. Photopolarimetric observations of the T Tauri star BM Andromedae V P Grinin E A Kolotilov A Rostopchina Astron. Astrophys. Suppl. Ser. 112 457 1995 1995A&AS..112..457G circumstellar matter polarization stars: individual (BM And) stars: pre-main sequence The results of photoelectric UBV observations of the T Tauri type variable BM And made during 1983-1991, as well as of simultaneous photopolarimetric UBVRI observations of this star for 1990-93 are given.
BM And photoelectric UBV observations JD Julian date d Vmag V magnitude mag u_Vmag Uncertainty flag (:) on V magnitude --- U-B U-B colour index mag u_U-B Uncertainty flag (:) on U-B --- B-V B-V colour index mag u_B-V Uncertainty flag (:) on B-V --- Data of simultaneous BM And and UBVRI photometry and polarimetry JD Julian day d Vmag V magnitude mag U-B U-B colour index mag u_U-B Uncertainty flag (:) on U-B --- B-V B-V colour index mag V-R V-R colour index mag V-I V-I colour index mag P(U) Degree of linear polarization in U passband % e_P(U) Error on P(U) % PA(U) Positional angle of polarization in U deg e_PA(U) Error on PA(U) deg P(B) Degree of linear polarization in B passband % e_P(B) Error on P(B) % PA(B) Positional angle of polarization in B deg e_PA(B) Error on PA(B) deg P(V) Degree of linear polarization in V passband % e_P(V) Error on P(V) % PA(V) Positional angle of polarization in V deg e_PA(V) Error on PA(V) deg P(R) Degree of linear polarization in R passband % e_P(R) Error on P(R) % PA(R) Positional angle of polarization in R deg e_PA(R) Error on PA(R) deg P(I) Degree of linear polarization in I passband % e_P(I) Error on P(I) % PA(I) Positional angle of polarization in I deg e_PA(I) Error on PA(I) deg Data of polarimetry of stars in the neighbourhood of BM And BD BD designation --- P(U) Degree of linear polarization in U passband % e_P(U) Error on P(U) % PA(U) Positional angle of polarization in U deg e_PA(U) Error on PA(U) deg P(B) Degree of linear polarization in B passband % e_P(B) Error on P(B) % PA(B) Positional angle of polarization in B deg e_PA(B) Error on PA(B) deg P(V) Degree of linear polarization in V passband % e_P(V) Error on P(V) % PA(V) Positional angle of polarization in V deg e_PA(V) Error on PA(V) deg P(R) Degree of linear polarization in R passband % e_P(R) Error on P(R) % PA(R) Positional angle of polarization in R deg e_PA(R) Error on PA(R) deg P(I) Degree of linear polarization in I passband % e_P(I) Error on P(I) % PA(I) Positional angle of polarization in I deg e_PA(I) Error on PA(I) deg Simona Mei CDS 1995 May 15 J_A+AS_112_457.xml uvby-beta photometry of 1017 stars earlier than G0 in the Centaurus-Crux-Musca-Chamaeleon direction J/A+AS/112/95 J/A+AS/112/95 uvby-beta photometry in Cen-Cru-Mus-Cha uvby-beta photometry of 1017 stars earlier than G0 in the Centaurus-Crux-Musca-Chamaeleon direction W J B Corradi G A P Franco Astron. Astrophys. Suppl. Ser. 112 95 1995 1995A&AS..112...95C dust, extinction ISM: individual (Southern Coalsack, Chamaeleon) stars: distances Stroemgren uvby{beta} photometry has been collected for a total of 1017 stars earlier than G0 lying in an area of the sky containing the Southern Coalsack, the Musca, and the Chamaeleon dark clouds. The targets were selected from the SAO star catalog, and the results give V, b-y, m_1_, c_1_, and {beta} on the standard systems, with overall rms errors for one observation of one star of 0.008mag , 0.004mag , 0.006mag , 0.009mag , and 0.011mag , respectively.
uvby-beta photometry of 1017 stars in the Centaurus-Crux-Musca-Chamaeleon direction SAO Star number in the SAO Catalog --- HD HD number --- Name Michigan two dimensional classification --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Vmag V magnitude mag e_Vmag rms uncertainty on Vmag 0.001mag n_Vmag "*" indicates error value larger than 99 --- b-y (b-y) colour index mag e_b-y rms uncertainty on b-y 0.001mag n_b-y "*" indicates error value larger than 99 --- m1 m1 colour index mag e_m1 rms uncertainty on m1 0.001mag n_m1 "*" indicates error value larger than 99 --- c1 c1 colour index mag e_c1 rms uncertainty on c1 0.001mag n_c1 "*" indicates error value larger than 99 --- o_Vmag Number of observations in uvby --- Beta Beta index mag e_Beta rms uncertainty on Beta 0.001mag n_Beta "*" indicates error value larger than 99 --- o_Beta Number of observations in Beta --- Patricia Bauer CDS 1995 Feb 13 franco@fisica.ufmg.br J_A+AS_112_95.xml Measurements of sky brightness at the Calar Alto Observatory J/A+AS/112/99 J/A+AS/112/99 Calar Alto Obs. sky brightness Measurements of sky brightness at the Calar Alto Observatory C Leinert P Vaisaenen K Mattila K Lehtinen Astron. Astrophys. Suppl. Ser. 112 99 1995 1995A&AS..112...99L J/A+AS/119/153 : La Silla Observatory sky brightness 1978-1988 (Mattila+ 1996) atmospheric effects site testing We report measurements of the sky brightness at the Calar Alto Observatory during 18 moonless nights in the years 1989, 1990, 1991, and 1993. Most of the measurements were performed in eight intermediate band filters between 350nm and 820nm. A set of measurements was obtained in the broad band UBVRI filters during three nights in 1990. Typically 10 to 20 readings were obtained each night for one or two fixed positions (fixed in {alpha}, {delta}), selected to be free of stars down to a limiting magnitude of about B=20. The sky brightnesses were calibrated using standard stars.
Narrow intermediate band surface photometry Date Date "DD/MM/YY" Filter Filter number number=1 For the narrow band data the FILTERS 01 ... 08 correspond to u (Stroemgren), 392nm, 403nm, b, 525nm, 580nm, 710nm, and 820nm, respectively. --- LST Local sideral time h 2.2mTel 2.2m telescope measurement ct/s 1.23mTel 1.23m telescope measurement ct/s SuBr Surface brightness (10-9 ergs/s/cm2/sr/Angstroem) number=2 See section 2.1. of the article for description of the derivation of intensities. Summary: the ratio of 1.23m/2.2m counts (and interpolation where needed) has been used. An abrupt change in the intensities during a night indicates a CHANGE OF TARGET; these are readily seen from Fig. 3. of the article. 10-11W/m2/sr/nm UBVRI broad band surface photometric data Date Date "DD/MM/YY" Filter Filter number number=1 For the broad band data the FILTERS 01 -- 05 correspond to Johnson bands U, B, V, R, and I, respectively. --- LST Local sideral time h 2.2mTel 2.2m telescope measurement ct/s 1.23mTel 1.23m telescope measurement ct/s SuBr Surface brightness number=2 See section 2.1. of the article for description of the derivation of intensities. Summary: the 2.2 m telescope was used as monitoring telescope, and its values are used directly. An abrupt change in the intensities during a night indicates a CHANGE OF TARGET; these are readily seen from Fig. 3. of the article. => The unit "S_10" (tenth magnitude stars per square degree) corresponds to the surface brightness which produces per square degree the flux of a 10th-magnitude star in the observed wavelength range. "S_10" End and beginning of astronomical twilight Date Date "DD/MM/YY" End End of Twilight (LST) h Beg Beginning of Twilight (LST) h Simona Mei CDS 1995 Mar 13 J_A+AS_112_99.xml Physical studies of asteroids XXIX. Photometry and analysis of 27 asteroids J/A+AS/113/115 J/A+AS/113/115 Photometry and analysis of 27 asteroids Physical studies of asteroids XXIX. Photometry and analysis of 27 asteroids C -I Lagerkvist A Erikson H Debehogne L Festin P Magnusson S Mottola T Oja G De Angelis I N Belskaya M Dahlgren M Gonano-Beurer J Lagerros K Lumme S Pohjolainen Astron. Astrophys. Suppl. Ser. 113 115 1995 1995A&AS..113..115L minor planets, asteroids In this paper photometry and analysis of 27 asteroids are presented. For the asteroids 21 Lutetia, 23 Thalia, 250 Bettina and 135 Hertha spin vector determinations were made. For asteroid 99 Dike we derived a rotation period of 10.35 hours and for 1280 Baillauda the period was found to be 12.6 hours. For 23 Thalia, 66 Maja and 250 Bettina the slope parameter was derived from the present data. The data are in a format "atlas 4" about which no explanation could be obtained from the authors. According to the authors, the data will be part of the Uppsala asteroid data base, described in the proceedings from the ACM 91 meeting in Belgirate edited by Milani et al (IAU symp. No 160), page 471; more details could be found at <http://www.astro.uu.se/planet/>
Francois Ochsenbein CDS 1995 May 19 Claes-Ingvar Lagerkvist <classe@chiron.astro.uu.se> J_A+AS_113_115.xml Observations of the Sun during 1994 with the astrolabe of Santiago J/A+AS/113/131 J/A+AS/113/131 Observations of the Sun during 1994 Observations of the Sun during 1994 with the astrolabe of Santiago F Noel Astron. Astrophys. Suppl. Ser. 113 131 1995 1995A&AS..113..131N astrometry Sun: general A program of solar observations at 30deg and 60deg zenith distance is in progress since 1990 with the modified Danjon astrolabe of Santiago. Results in right ascension, parameter Y and apparent semi-diameter of the Sun obtained with the astrolabe at both zenith distances during 1994, are available.
Sun observations at 30deg zenith distance Sun observations at 60deg zenith distance Date Date (year-1900,month,day) "YYMMDD" MJD Modified Julian day (JD-2400000.5) d EUB Zenith distance residual east upper border arcsec ELB Zenith distance residual east lower border arcsec WLB Zenith distance residual west lower border arcsec WUB Zenith distance residual west upper border arcsec dAlpha Right ascension (O-C) s e_dAlpha Sigma of dAlpha s Y Y=Zenith distance (Observed-Adopted) + Declination(O-C)cos S (Sun's parallactic angle). arcsec dD dD=Sun semi-diameter (O-C) arcsec e_dD Sigma of dD and Y arcsec DR Observed Sun semi-diameter reduced to the AU. arcsec Simona Mei CDS 1995 Apr 26 J_A+AS_113_131.xml Velocity dispersions for elliptical galaxies I. First set of measurements J/A+AS/113/151 J/A+AS/113/151 Velocity dispersions for elliptical galaxies Velocity dispersions for elliptical galaxies I. First set of measurements H Di Nella A M Garcia R Garnier G Paturel Astron. Astrophys. Suppl. Ser. 113 151 1995 1995A&AS..113..151D catalogs galaxies: distances and redshifts galaxies: elliptical and lenticular, cD galaxies: kinematics and dynamics methods: data analysis Measurements of central velocity dispersions and heliocentric radial velocities are presented for 94 field galaxies. Among these, 5 new radial velocities and 80 new central velocity dispersions are obtained. Reduction was performed independently by cross-correlation, Fourier-quotient and Fourier-correlation-quotient methods.
Results from Cross-Correlation, Fourier-Quotient and Fourier-Correlation-Quotient methods PGC PGC number (Principal Galaxies Catalog) --- Name Alternative name in a given hierarchy: NGC, IC, UGC, MCG --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec MType Morphological type description according to LEDA database (2) number=1 The classification is made according to the Hubble system --- HRV Mean heliocentric radial velocity from literature (LEDA database) number=2 The measurements are available through the free access Lyon-Meudon Extragalactic Database (LEDA) via telnet lmc.univ-lyon1.fr, login: leda <telnet://leda@lmc.univ-lyon1.fr> km/s VelDisp Mean central velocity dispersion from literature (LEDA database) number=2 The measurements are available through the free access Lyon-Meudon Extragalactic Database (LEDA) via telnet lmc.univ-lyon1.fr, login: leda <telnet://leda@lmc.univ-lyon1.fr> km/s Source Bibliographic source code number=3 a) V,S2; b) D1: c) B,D2,D3,S1,T; d) T,M1; e) D1,D3; f) S3; g) M2,D1; h) D1,D2. B Bender et al., 1994 =1994MNRAS.269..785B D1 Dalle Ore et al. 1991 =1991ApJ...366...38D D2 Davies et al., 1987 =1987ApJS...64..581D D3 Dressler, Sandage, 1983 =1983ApJ...265..664D M1 Malumuth, Kirshner, 1985 =1985ApJ...291....8M M2 Minkowski, 1962 =1962IAUS...15..112M S1 Schechter, 1980 =1980AJ.....85..801S S2 Schechter, 1983 =1983ApJS...52..425S S3 Smith et al., 1990 =1990ApJ...356..399S T Tonry, Davis, 1981 =1981ApJ...246..666T V Van der Kruit, Freeman, 1984. =1984ApJ...278...81V --- CCHRV Heliocentric velocity from the cross-correlation method km/s CCVelDisp Central velocity dispersion from the cross-correlation method km/s FQHRV Heliocentric velocity from the Fourier quotient method km/s FQVelDisp Central velocity dispersion from the Fourier quotient method km/s FCQHRV Heliocentric velocity from the Fourier correlation quotient method km/s FCQVelDisp Central velocity dispersion from the Fourier correlation quotient km/s Ident Identification of the observing run where the measurement was obtained number=4 Observing runs at OHP observatory. 1 Apr 22-30, 1992 OHP1 2 Nov 16-24, 1992 OHP2 3 Jan 22-Feb 1, 1993 OHP3 4 Sep 16-23, 1993 OHP4 5 Oct 15-21, 1993 OHP5 6 Mar 14-21, 1994 OHP6 -------------------------------- Technical characteristics of the CARELEC spectrograph used with the 193 cm reflector of the OHP: ---------------------------------------------------------------------------- OHP1 OHP2 OHP3 OHP4 OHP5-OHP6 ---------------------------------------------------------------------------- Grating (mm-1) 600 600 1200 1200 1200 Blaze (A) 5000 5000 4000 7000 4000 Filter GG375 GG375 none OG590 none Dispersion (Amm-1) 66 66 33 33 33 Resolution (Apixel-1) 1.78 1.78 0.89 0.89 0.89 Wavelegth coverage (A) 5099-6056 5099-6056 5727-6205 5727-6205 5727-6205 Central Wavelength (A) 5577 5577 5966 5966 5966 Slit width (arcsec) 2.4 2.4 2.3 2.1 2.3 Slit length (arcsec) 344 344 344 344 344 ---------------------------------------------------------------------------- --- S/N Signal/Noise ratio --- Mean observed heliocentric radial velocities and central velocity dispersions with their mean errors. PGC PGC number (Paturel et al. 1989) --- HRV Mean heliocentric radial velocity from this paper km/s e_HRV Mean error on the mean heliocentric radial velocity calculated from different measurements km/s VelDisp Mean central velocity dispersion from this paper km/s u_VelDisp Uncertainty flag (values smaller than the pixel resolution in km/s) --- e_VelDisp Mean error on the mean central velocity dispersion km/s Simona Mei CDS 1995 Jun 08 J_A+AS_113_151.xml A High Spectral Resolution Atlas of the Balloon Ultraviolet Spectrum of the Sun: 1950-2000 Angstroems J/A+AS/113/237 J/A+AS/113/237 Ultraviolet Spectrum of the Sun A High Spectral Resolution Atlas of the Balloon Ultraviolet Spectrum of the Sun: 1950-2000 Angstroems D Samain Astron. Astrophys. Suppl. Ser. 113 237 1995 1995A&AS..113..237S line: identification Sun: atmosphere Sun: atmospheric motions Sun: UV radiation An ultraviolet atlas of the solar spectrum with a spectral resolution of 15mA in the region 1948-2000A is presented. It is the first part of the spectra recorded on the quiet Sun between 1900 and 2130A. Measurements were performed from a balloon-borne instrumentation flown at an altitude of 39km. The wavelength atlas with a list of about 550 lines has been synthesized from data at center of the Sun ({mu}=1) and at {mu}=0.89, smoothed out over an area of 30 arcsec. The wavelength scale is given with respect to the average solar spectrum. Tracings are presented at {mu}=0.89, with an intensity scale adjusted in absolute values on the level of the continuum near 2000A.
Observed wavelengths, laboratory values and identifications SpOrd Spectrum order --- SolLam Wavelength determination of all solar and telluric lines measurable on the spectrum number=1 All wavelengths are given in the vacuum, according to usage below 2000 A. As underlined in the A&A publication, an average shift of 7mA is to be added to the measured value of the telluric lines for a proper comparison with their laboratory wavelengths. 0.1nm n_SolLam See Note number=2 When 'a' these lines correspond to features not separated in the observed spectrum. When we tried to take these wavelengths as references in the wavelength tabulation, we have compared the average measured wavelength to the arithmetic average of the two laboratory wavelengths. --- Intens Intensity of the line in an arbitrary scale from 0 to 9 number=3 Approximately representing the degree of absorption at the center of the line with respect to the intensity level outside of the line; 0 is a line barely detectable. --- n_Intens When '?' uncertain value --- Type Acronyms for the type of line number=4 W: wide line(50-100mA) VW: very wide line(>100mA) b: blend d: double line e: emission line T: terrestrial O2 line(no indication = solar line) T*: terrestrial O2 reference line S*: solar reference line (S*)/(T*): solar/telluric reference line ejected --- Identif Possible element responsible for the observed line number=5 Laboratory lines whose wavelength differences with our solar determinations are not lower than 10 m, have not been retained generally, unless the laboratory uncertainty exceeds that value or the feature observed is very wide. In the case of telluric lines, whose features listed here are all due to O2, notation of the transition is given instead of the name of the element. To point out the disturbed regions of the solar spectrum, we have reported all the laboratory wavelengths of known lines belonging to the O2 Shuman-Runge system and encompassed by the spectral interval 1948-2000. However, for many weak lines (like the bands 5-1 and 4-1) correspondence with observed values in the atlas is often given only for the record. --- LabLam Laboratory wavelength 0.1nm n_LabLam When 'St' the line is used or recommended as reference wavelength standard --- r_LabLam References of the wavelength sources number=6 J: Junkes et al., 65 K: Kelly, 87 KE: Kaufman & Edlen, 74 KRA: Kaufman et al., 66 M: Moore, 62 MCA: MacCabe & MacAllister, 82 R: Radziemski et al., 67 WA: Wilkinson & Andrew, 63 WS: Weeks & Simpson, 67 Y: Yoshino et al., 84 --- DLam Difference between the observed wavelength and the laboratory wavelength: dlambda=lambda(Sun or O2) - lambda(lab) 0.1nm Simona Mei CDS 1995 Jun 08 J_A+AS_113_237.xml Abundances and velocities for open and globular cluster giants: The data J/A+AS/113/299 J/A+AS/113/299 Abundances and velocities for cluster giants Abundances and velocities for open and globular cluster giants: The data D Minniti Astron. Astrophys. Suppl. Ser. 113 299 1995 1995A&AS..113..299M Galaxy: abundances globular clusters: general stars: abundances We present a large dataset consisting of giants in the field, and in open and globular clusters. A total of 122 giants were observed in the fields of 8 open clusters. A total of 342 giants were observed in the fields of 25 globular clusters. A total of 36 field stars with well known abundances and luminosities were also observed. Table 8 lists the spectral indices measured for the giants observed with the Argus and Red Channel spectrographs during 1991 and 1992. The central and continuum passbands for these indices are defined in Table 6.
Definition of Spectral Indices SpInd Spectral index --- LLpb Lower limit of the passband 0.1nm ULpb Upper limit of the passband 0.1nm LLc1 Lower limit of continuum 1 0.1nm ULc1 Upper limit of continuum 1 0.1nm LLc2 Lower limit of continuum 2 0.1nm ULc2 Upper limit of continuum 2 0.1nm Spec Species --- Crit Criterion --- Spectral Indices for open and globular cluster giants Cluster Cluster name --- Star Star name --- Mg Spectral index Mg number=1 As defined in table 6 mag Hbeta Spectral index Hbeta number=1 As defined in table 6 mag Fe492 Spectral index Fe492 number=1 As defined in table 6 mag Fe498 Spectral index Fe498 number=1 As defined in table 6 mag Fe50 Spectral index Fe50 number=1 As defined in table 6 mag Fe52 Spectral index Fe52 number=1 As defined in table 6 mag Fe53 Spectral index Fe53 number=1 As defined in table 6 mag Fe54 Spectral index Fe54 number=1 As defined in table 6 mag Mg1 Spectral index Mg1 number=1 As defined in table 6 mag Mg2 Spectral index Mg2 number=1 As defined in table 6 mag Mgb Spectral index Mgb number=1 As defined in table 6 mag MgH Spectral index MgH number=1 As defined in table 6 mag Simona Mei CDS 1995 Apr 03 J_A+AS_113_299.xml Distance measurements of Lynds galactic dark nebulae J/A+AS/113/325 J/A+AS/113/325 Distance measurements of Lynds Nebulae Distance measurements of Lynds galactic dark nebulae J Hilton J F Lahulla Astron. Astrophys. Suppl. 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Italiana, 40, 75 Wilking B.A., Blackwell J.H., Mundy L.G., 1990, AJ, 100, 758 Witt A.N., Walker G.A.H., Bohlin R.C., Stecher T.P., 1982, ApJ, 261, 492 Wu Y., Zhou S., Evans 11 N.J., 1992, ApJ, 394, 196 Xie T., Goldsmith P.F., 1990, ApJ, 359, 378 Young J.S., Goldsmith P.F., Langer W.D., Wilson R.W., Carlson E.R., 1982, ApJ, 261, 513 astronomical data bases: miscellaneous dust, extinction ISM: clouds ISM: general A literature search has been carried out in order to obtain a distance table for the Lynds galactic nebulae which in the main have been cited in Astronomy and Astrophysics Abstracts between 1980 and 1984. Inevitably this list cannot be without omission and a request is made for any further information which could lead to the publication of a more complete compilation.
Lynds galactic dark nebulae LDN Lynds cloud number --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (1950) h RAm Right ascension (1950) min DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin Names Alternative designations mainly for the Lynds clouds which are also in the Barnard catalogue (1927) --- Nref Number of references to the Lynds fields from 1980 to 1994 as listed in the SIMBAD data base --- Distance measurements LDN Lynds cloud number --- Ref Reference number --- Dist3 Distance value (when n_Dist3 is '-') pc n_Dist3 When '-' there are three values listed for the distance --- Dist2 Distance value (when n_Dist2 is '-') pc n_Dist2 When '-' there are two or 3 values for the distance; when '<' Dist is an upper limit --- Dist Distance value pc n_Dist '*' indicates different estimated distances; 'k' indicates kinematic distances --- e_Dist Mean error on Dist pc Refs References for the distance number=1 If two references are quoted for one distance, the first given provides a distance from the work of the second. Sometimes several authors quote the same distance value and under these circumstances one of them is normally included in table1b --- Simona Mei CDS 1995 Apr 21 J_A+AS_113_325.xml H {alpha} velocity fields and rotation curves of galaxies in clusters. III. Nine galaxies in DC 1842-63 J/A+AS/113/35 J/A+AS/113/35 Rotation curves of galaxies in DC 1842-63 H {alpha} velocity fields and rotation curves of galaxies in clusters. III. Nine galaxies in DC 1842-63 P Amram J Boulesteix M Marcelin C Balkowski V Cayatte W T Sullivan Iii Astron. Astrophys. Suppl. Ser. 113 35 1995 1995A&AS..113...35A galaxies: clusters: general galaxies: clusters: individual (DC 1842-63) galaxies: ISM galaxies: kinematics and dynamics H {alpha} maps, velocity contour maps and rotation curves are presented for nine galaxies in the Southern cluster DC 1842-63. These data have been obtained from the two-dimensional H {alpha} observations at the 3.60m ESO Telescope equipped with CIGALE, a scanning Fabry-Perot interferometer.
Detailed information about the rotation curves Galaxy Galaxy --- R Mean radius on the major axis of the annulus for which the rotational velocity is calculated arcsec Napp Number of points with measurable velocities in the annulus for the approaching side of the galaxy --- Vapp Weighted average velocity calculated from the Napp points km/s e_Vapp Error in Vapp (+/- r.m.s.) km/s Nrec Number of points with measurable velocities in the annulus for the receding side --- Vrec Weighted average velocity calculated from the Nrec points km/s e_Vrec Error in Vrec (+/- r.m.s.) km/s Ntot Total number of velocity points N=Napp+Nrec --- Vtot Weighted average velocity computed from both sides km/s e_Vtot Error in Vtot (+/- r.m.s.) km/s Simona Mei CDS 1995 Apr 13 J_A+AS_113_35.xml High-precision study of proper motions and membership of 924 stars in the central region of Praesepe. J/A+AS/113/419 J/A+AS/113/419 Proper motions in Praesepe High-precision study of proper motions and membership of 924 stars in the central region of Praesepe. J J Wang L Chen J H Zhao P F Jiang Astron. Astrophys. Suppl. Ser. 113 419 1995 1995A&AS..113..419W astrometry open clusters and associations: individual (Praesepe) High-precision proper motions for 257 and 296 stars in a 90x90' region centered on BD+20 2170 were obtained from seven plates taken with the 40cm refractor (f=6895mm) at Zo-Se station of Shanghai Observatory with six AC plates and the stellar positions in Russell's (1976, Ph.D. Thesis, University of Pittsburgh) catalogue, respectively. Combining with the data given by Klein-Wassink, Jones (1971), Artyukhina, and Jones & Cudworth, these proper motions give a sample of 924 stars in the region mentioned above. With membership probabilities estimated by an improved maximum likelihood method, a very good sample of 198 members is obtained with proper motion accuracies ranging from +/-0.2 to +/-5.0mas/yr, of which 60 per cent are better than +/-1.0mas/yr, and the completeness nearly down to B=15.5.
Combined data of proper motions for 924 stars in the central region of the Praesepe and their membership Number Ordinal number --- NRuss Russell's (1976) number --- NKW Klein-Wassink's (1927) number --- NArt Artyukhina's (1971) number --- NJC Jones & Cudworth's (1983) number --- n_Number AC star is indicated with '*' --- Mag V magnitude or B magnitude when there is a 'B' in the next column mag n_Mag When 'B' given magnitude is B magnitude --- B-V B-V colour index mag 1Remarks Remarks: see Note number=1 P - photoelectric G - photographic --- 2Remarks Remarks: see Note number=2 C - combined from Johnson(1952), Upgren et al.(1979), Weis(1981), and Stauffer(1982) G - Gotz's (1984) J - Jones & Cudworth's (1983) R - Russell's (1976) --- 3Remarks Remarks: see Note number=3 B - s.e. less than 0.01 G - s.e. from 0.01 to 0.04 F - s.e. from 0.04 to 0.08 P - s.e. greater than 0.08 --- RAh Right ascension for the equinox J2000.0 and epoch 1986.17 h RAm Right ascension for the equinox J2000.0 and epoch 1986.17 min RAs Right ascension for the equinox J2000.0 and epoch 1986.17 s DE- Declination sign --- DEd Declination for the equinox J2000.0 and epoch 1986.17 deg DEm Declination for the equinox J2000.0 and epoch 1986.17 arcmin DEs Declination for the equinox J2000.0 and epoch 1986.17 arcsec pmRA Proper motion component in right ascension reduced into the great circle 0.1mas/yr e_pmRA Standard error of proper motion in RA 0.1mas/yr pmDE Proper motion component in declination 0.1mas/yr e_pmDE Standard error of proper motion in DE 0.1mas/yr Prob Membership probability --- Member Membership judgement:'1' if probability is less than 0.36, '0' otherwise --- n_Member Notes about previous membership judgements, note number=4 K - member by Klein-Wassink (1927) A - member by Artyukhina (1971) Figures - non-zero membership probability by Jones & Cudworth (1983) --- Simona Mei CDS 1995 Nov 21 Wang Jiaji <xytan@fudan.ihep.ac.cn> J_A+AS_113_419.xml Semiregular variables of types SRa and SRb. New JHKL'M-photometry for 44 stars. J/A+AS/113/441 J/A+AS/113/441 JHKL'M-photometry for 44 stars Semiregular variables of types SRa and SRb. New JHKL'M-photometry for 44 stars. F Kerschbaum Astron. Astrophys. Suppl. Ser. 113 441 1995 1995A&AS..113..441K II/177 : Fouque et al., 1992, NIR photometry of a sample of IRAS Point Sources J/A+AS/99/31 : Guglielmo et al., 1993, 106 new IR Carbon stars in the IRAS Point Source Catalog. J/A+AS/106/397 : JHKL'M-photometry for 200 stars Fouque P., Le Bertre T., Epchtein N., Guglielmo F., Kerschbaum F., =1992A&AS...93..151F (Catalogue: <II/177>) Guglielmo F., Epchtein N., Le Bertre T., Fouquet P., Hron J., Kerschbaum F., Lepine J.R.D., =1993A&AS...99...31G Kerschbaum F. and Hron J., =1992A&A...263...97K (Paper I) Kerschbaum F. and Hron J., =1994A&AS..106..397K infrared: stars stars: AGB and post-AGB stars: mass-loss stars: variables: general This paper supplements Kerschbaum and Hron (1994), where new JHKL'M observations of 200 Semiregular variables of types SRa and SRb were presented with additional 44 near infrared observations and 5 literature data sets. The total sample was defined in Kerschbaum & Hron (1992, Paper I) by means of a certain limit in bolometric magnitude. From the sample of 350 objects, 303 now have near infrared (NIR) photometry. In total 339 datasets are available because of some multiple observations. A detailed analysis of the whole dataset will be presented in a forthcoming paper.
Near-infrared photometry GCVS4 GCVS4 name --- IRAS IRAS (Catalogue <II/125>) name --- Vtype Variability type --- u_Vtype Uncertainty flag on variability type --- Chem Chemistry code number=1 code opt. spectra / IRAS-LRS vulgo ---------------------------------------------------- 0 no information 1 C/no 2n or 3n; ?/4n `C-rich' 2 C/2n or 3n 3 R/any n 4 MS or S/any n `S-stars' 5 M/4n 6 M/no 4n; ?/2n or 3n `O-rich' --- SRV SRV code number=2 b: blue; r: red; M: Myra-like. These types of O-rich Semi Regular Variables are defined in Kerschbaum and Hron 1992 and 1994. --- JD Julian day d n_JD Approximative date number=3 A: 13-07-89 to 20-07-89; B: 10-08-89 to 16-08-89; C: 31-01-91 to 09-02-91. --- Jmag J magnitude mag Hmag H magnitude mag Kmag K magnitude mag L'mag L' magnitude mag Mmag M magnitude mag Obs Observatory code number=4 M: ESO, new, stars=24; I: IAC, new, stars=20; F: ESO, Fouquet et al. 1992, stars=4; G: ESO, Guglielmo et al. 1993, stars=1. --- Simona Mei CDS 1995 May 15 J_A+AS_113_441.xml Photometric observations of pre-main sequence objects J/A+AS/113/473 J/A+AS/113/473 Photometric observations of PMS objects Photometric observations of pre-main sequence objects M Fernandez Astron. Astrophys. Suppl. Ser. 113 473 1995 1995A&AS..113..473F stars: formation stars: pre-main sequence We present the observational data of a photometric monitoring of 24 pre-main sequence objects: T Tauri stars, Ae/Be Herbig stars and some unclassified objects. Observations were carried out from July 1988 to August 1992, using the UBV(RI)_c system. Variability with time scales from days to years and amplitudes in the V band larger than 0.1 mag is found for a part of this sample. The analysis of the possible causes of this variability are discussed in separate papers (Fernandez & Eiroa 1995a,b).
Photometric observations of V594 Cas (HBC 330) - C2 V594 Cas Photometric observations of LkHalpha 264 (HBC 10) - C4 LkHalpha 264 Photometric observations of LkHalpha 325 (HBC 11) - C3 LkHalpha 325 Photometric observations of LkHalpha 330 (HBC 20) - C3 LkHalpha 330 Photometric observations of V773 Tau (HBC 367) - C2 V773 Tau Photometric observations of AS 205 (HBC 254) - C2 AS 205 Photometric observations of V1221 Oph (HBC 270) - C1 V1221 Oph Photometric observations of VV Ser (HBC 282) - C1 VV Ser Photometric observations of AS 310 (HBC 284) - C2 AS 310 Photometric observations of AS 353 A and B (HBC 292 and HBC 685) Photometric observations of WW Vul (HBC 686) - C2 WW Vul Photometric observations of LHalpha 483-41 (HBC 293) - C1 LHalpha 483-41 Photometric observations of LkHalpha 228 (HBC 295) - C2 LkHalpha 228 Photometric observations of LkHalpha 191 (HBC 301) - C1 LkHalpha 191 Photometric observations of V1331 Cyg (HBC 302) - C2 V1331 Cyg Photometric observations of LkHalpha 321 (HBC 303) - C1 LkHalpha 321 Photometric observations of LkHalpha 324 (HBC 305) - C4 LkHalpha 324 Photometric observations of LkHalpha 349 (HBC 308) - C5 LkHalpha 349 Photometric observations of BD +65 1637 (HBC 730) - C2 BD +65 1637 Photometric observations of LkHalpha 234 (HBC 309) - C2 LkHalpha 234 Photometric observations of LkHalpha 233 (HBC 313) - C7 LkHalpha 233 Photometric observations of DI Cep (HBC 315) - C4 DI Cep Photometric observations of MWC 1080 (HBC 317) - C3 MWC 1080 Photometric observations of BM And (HBC 318) - C4 BM And JD-2440000 Julian Date (-2440000) d Vmag Difference in the V band mag (B-V) Difference in the (B-V) colour index mag (U-B) Difference in the (U-B) colour index mag (V-R) Difference in the (V-R) colour index mag (V-I) Difference in the (V-I) colour index mag Matilde Fernandez, Simona Mei CDS 1995 May 17 J_A+AS_113_473.xml RR Lyrae stars and Baade-Wesselink method. V. Photometric and radial velocity measurements of BH Peg, RX Eri, SS Leo, UU Vir and X Ari J/A+AS/113/483 J/A+AS/113/483 Photometric and radial velocity of RRLyr stars RR Lyrae stars and Baade-Wesselink method. V. Photometric and radial velocity measurements of BH Peg, RX Eri, SS Leo, UU Vir and X Ari D Carrillo G Burki M Mayor M Burnet P Lampens B Nicolet Astron. Astrophys. Suppl. Ser. 113 483 1995 1995A&AS..113..483C stars: individual (BH Peg, RX Eri, SS Leo, UU Vir, X Ari) stars: variables: other Almost simultaneous measurements in the Geneva seven-colour photometric system and in radial velocities with the spectrometer CORAVEL for five RR Lyrae field stars were obtained in order to apply the Baade-Wesselink method to this kind of variable stars. In this paper the observational data on these stars are presented; the analysis of their physical parameters will be published in the forthcoming paper of the series.
Photometric measurements of BH Peg Photometric measurements of SS Leo Photometric measurements of UU Vir Photometric measurements of X Ari NMeas Number of measurements --- JD Heliocentric Julian day d AirMass Air mass --- Vmag V magnitude mag w_Vmag Weight of V magnitude --- U-B Geneva colour index U-B mag V-B Geneva colour index V-B mag B1-B Geneva colour index B1-B mag B2-B Geneva colour index B2-B mag V1-B Geneva colour index V1-B mag G-B Geneva colour index G-B mag w_colours Weight of colours --- Radial velocity measurements of BH Peg Radial velocity measurements of SS Leo Radial velocity measurements of UU Vir NMeas Number of measurements --- JD Heliocentric Julian day d RV Radial velocity km/s e_RV Error on radial velocity km/s Simona Mei CDS 1995 Jun 07 J_A+AS_113_483.xml A catalogue of associations between IRAS sources and S stars J/A+AS/113/51 J/A+AS/113/51 Catalogue of associations IRAS and S stars A catalogue of associations between IRAS sources and S stars P S Chen H Gao A Jorissen Astron. Astrophys. Suppl. Ser. 113 51 1995 1995A&AS..113...51C II/125 : IRAS Catalogue of point sources (IRAS-PSC) III/168 : General Catalog of S Stars, second edition (Stephenson 1984) catalogs infrared: stars stars: AGB, S Cross identifications between the General Catalogue of Galactic S Stars (GCGSS), the IRAS Point Source Catalogue (PSC), and the Guide Star Catalogue (GSC) are presented. The purpose of the present catalogue is i) to provide a clean sample of S stars with far-IR data, and ii) to provide accurate GSC positions for S stars, superseding those listed in the GCGSS. The IRAS colour-colour diagram and the galactic distribution of S stars associated with an IRAS source are presented. Several S stars having extended images in at least one IRAS band have also been identified.
Association between IRAS sources and S stars Rejected associations GCGSS GCGSS or Stephenson (1990) number number=1 GCGSS: General Catalogue of Galactic S Stars, Stephenson C.B., 1984, Publ. Warner and Swasey Obs. 3,1 <III/168> Stephenson C.B. =1990AJ....100..569S --- n_GCGSS If S flag is present, star belongs to Stephenson's (1990) supplementary list number=1 GCGSS: General Catalogue of Galactic S Stars, Stephenson C.B., 1984, Publ. Warner and Swasey Obs. 3,1 <III/168> Stephenson C.B. =1990AJ....100..569S --- RAh GCGSS right ascension (1950) h RAm GCGSS right ascension (1950) min RAs GCGSS right ascension (1950) s n_RAs When '*' the seconds were indicated as tenths of minutes in the original table --- DE- Declination sign --- DEd GCGSS declination (1950) deg DEm GCGSS declination (1950) arcmin DEs GCGSS declination (1950) arcsec n_DEs When '*' the arcseconds were indicated as tenths of arcminutes in the original table --- GCGSSmag GCGSS magnitude, either V or B mag n_GCGSSmag When 'B' GCGSS magnitude is B --- RA2m GSC right ascension (1950) min RA2s GSC right ascension (1950) s DE2m GSC declination (1950) arcmin DE2s GSC declination (1950) arcsec GSCmag GSC magnitude, either V or B mag n1_GSCmag When 'B' GSC magnitude is B --- n2_GSCmag When 'v' GSC magnitude is variable --- IRAS IRAS PSC entry --- RA3s IRAS right ascension (1950) s DE3m IRAS declination (1950) arcmin DE3s IRAS declination (1950) arcsec R1 log(25.F12/12.F25)/log(25/12), where F12 and F25 are the 12 and 25um IRAS fluxes --- n_R1 If present, at least one flux is of quality 2 in IRAS --- R2 log(60.F25/25.F60)/log(60/25), where F25 and F60 are the 25 and 60um IRAS fluxes --- n1_R2 If present, at least one flux is of quality 2 --- SpIR IR spectral class, according to the letter codes defined by Volk & Cohen number=2 Volk K. and Cohen M. =1989AJ.....98..931V --- LRS LRS spectral class --- Refs References to near IR photometry number=3 a: Catchpole R.M. et al., =1979SAAOC...1...61C b: Chen P.S. et al., 1988, =1988A&AS...72..239C c: Chen P.S. et al., 1991, =1991AcASn..32...10C d: Noguchi K. et al., 1986, =1986PASJ...38..811N e: Noguchi K. et al., 1991, =1991PASJ...43..311N --- Ass Associations with other catalogues number=4 HD (listed bare numbers); DM, General Catalogue of Variable Stars, Catalogue of Suspected Variable Stars, Two-Micron Sky Survey, Dearborn Observatory, Catalogue of Faint Red Stars --- Flag Flag number=5 As described in the paper. Note that: 'a' indicates two or more GSC stars fall within the IRAS error ellipses; their position and magnitude are given on the following line(s); '*' means that there is a remark concerning that star in the remark file corresponding at the table --- Suspected associations GCGSS Stephenson number (see Note (1) in table1) --- n_GCGSS (see Note (1) in table1) --- RAh GCGSS right ascension (1950) h RAm GCGSS right ascension (1950) min RAs GCGSS right ascension (1950) s n_RAs When '*' the seconds were indicated as tenths of minutes in the original table --- DE- Declination sign --- DEd GCGSS declination (1950) deg DEm GCGSS declination (1950) arcmin DEs GCGSS declination (1950) arcsec n_DEs When '*' the arcseconds were indicated as tenths of arcminutes in the original table --- GCGSSmag GCGSS magnitude, either V or B mag n_GCGSSmag When 'B' GCGSS magnitude is B --- IRAS IRAS PSC entry --- RA3s IRAS right ascension (1950) s DE3s IRAS declination (1950) arcsec R1 log(25 F12/12 F25)/log(25/12), where F12 and F25 are the 12 and 25um IRAS fluxes --- n_R1 If present, at least one flux is of quality 2 --- R2 log(60 F25/25 F60)/log(60/25), where F25 and F60 are the 25 and 60um IRAS fluxes --- n_R2 If present, at least one flux is of quality 2 --- SpIR IR spectral class, according to the letter codes defined by Volk & Cohen (Note (2) in table1) --- LRS LRS spectral class --- Refs References to near IR photometry (Note (3) in table1) --- Ass Associations with other catalogues (Note (4) in table1) --- Flag Flag (Note (5) in table1) --- Remarks to table1 and table2 GCGSS GCGSS number (Note (1) in table1) --- Text Remarks --- Remarks to table3 GCGSS GCGSS or Stephenson number (Note (1) in table1) --- n_GCGSS (see Note (1) in table1) --- IRAS IRAS PSC entry --- Text Remarks --- Possibly extended sources Sources contaminated by cirrus or nearby sources GCGSS GCGSS or Stephenson number (Note (1) in table1) --- n_GCGSS (see Note (1) in table1) --- IRAS IRAS PSC entry --- ses1 IRAS PSC small extended structure flag --- Text Text of remarks --- Simona Mei CDS 1995 Apr 13 J_A+AS_113_51.xml CCD astrometric observations of Uranian satellites J/A+AS/113/557 J/A+AS/113/557 Uranian satellites CCD astrometric observations of Uranian satellites C H Veiga R Vieira Martins Astron. Astrophys. Suppl. Ser. 113 557 1995 1995A&AS..113..557V astrometry planets and satellites: individual (satellites of Uranus) Astrometric positions of the five largest satellites are given for the oppositions of Uranus for the years 1989 to 1994. These positions were measured on 368 CCD frames obtained at the Cassegrain focus of a 1.6-m reflector. They are compared with the theoretically calculated positions from GUST86 (Laskar & Jacobson 1987). The observed minus calculated residuals referred to Oberon have standard deviations of the order of 0.05" for the three greatest Uranian satellites and 0.07" for Miranda. These residuals are comparable to the best available in the literature.
List of observed positions of the Uranian satellites Year Year of observation --- Month Month of observation --- UTCday UTC day of observation d XposM Miranda X position referred to Oberon number=1 The reference system is defined by the mean equator and equinox 1950.0 arcsec YposM Miranda Y position referred to Oberon number=1 The reference system is defined by the mean equator and equinox 1950.0 arcsec XposA Ariel X position referred to Oberon number=1 The reference system is defined by the mean equator and equinox 1950.0 arcsec YposA Ariel Y position referred to Oberon number=1 The reference system is defined by the mean equator and equinox 1950.0 arcsec XposU Umbriel X position referred to Oberon number=1 The reference system is defined by the mean equator and equinox 1950.0 arcsec YposU Umbriel Y position referred to Oberon number=1 The reference system is defined by the mean equator and equinox 1950.0 arcsec XposT Titania X position referred to Oberon number=1 The reference system is defined by the mean equator and equinox 1950.0 arcsec YposT Titania Y position referred to Oberon number=1 The reference system is defined by the mean equator and equinox 1950.0 arcsec Simona Mei CDS 1995 Jun 07 J_A+AS_113_557.xml Stark broadening of the NV 6f,g,h-7f,g,h,i line complex J/A+AS/113/579 J/A+AS/113/579 Stark broadening Stark broadening of the NV 6f,g,h-7f,g,h,i line complex T Schoening Astron. Astrophys. Suppl. Ser. 113 579 1995 1995A&AS..113..579S atomic data line: profiles plasmas stars: abundances Tables of Stark broadening profiles for the N V 6f, g, h-7f, g, h, i line complex at 4945A have been generated. Modern close-coupling techniques are used for the electron broadening while the important influence of perturbing ions is included within the framework of the model microfield method. Comparison has been made with the results of line formation calculations using approximate formulae for the Stark profiles.
e- and H+ perturbers (+ Doppler + Radiation) Ne Electron density cm-3 DeltaLambda0 Wavelength of intensity maximum number=1 Delta lambda = Delta lambda0 + delta lambda where Delta lambda denotes the wavelength detuning from line centre (6h-7i at 494.5 nm), Delta lambda0 the wavelength separation (relative to the line centre) of prominent intensity maxima and delta lambda the detuning from the nearest intensity maximum. 0.1nm deltaLambda Detuning from intensity maximum number=1 Delta lambda = Delta lambda0 + delta lambda where Delta lambda denotes the wavelength detuning from line centre (6h-7i at 494.5 nm), Delta lambda0 the wavelength separation (relative to the line centre) of prominent intensity maxima and delta lambda the detuning from the nearest intensity maximum. 0.1nm S2 Intensity (Temperature T= 2.10+4 K) number=2 Normalized intensity in frequency units, e- and H+ perturbers (with thermal Doppler broadening and radiative damping). Hz-1 S4 Intensity (Temperature T= 4.10+4 K) number=2 Normalized intensity in frequency units, e- and H+ perturbers (with thermal Doppler broadening and radiative damping). Hz-1 S8 Intensity (Temperature T= 8.10+4 K) number=2 Normalized intensity in frequency units, e- and H+ perturbers (with thermal Doppler broadening and radiative damping). Hz-1 S16 Intensity (Temperature T= 16.10+4 K) number=2 Normalized intensity in frequency units, e- and H+ perturbers (with thermal Doppler broadening and radiative damping). Hz-1 e- and H+ perturbers (Stark only) Ne Electron density cm-3 DeltaLambda0 Wavelength of intensity maximum number=1 Delta lambda = Delta lambda0 + delta lambda where Delta lambda denotes the wavelength detuning from line centre (6h-7i at 494.5 nm), Delta lambda0 the wavelength separation (relative to the line centre) of prominent intensity maxima and delta lambda the detuning from the nearest intensity maximum. 0.1nm deltaLambda Detuning from intensity maximum number=1 Delta lambda = Delta lambda0 + delta lambda where Delta lambda denotes the wavelength detuning from line centre (6h-7i at 494.5 nm), Delta lambda0 the wavelength separation (relative to the line centre) of prominent intensity maxima and delta lambda the detuning from the nearest intensity maximum. 0.1nm F2 Intensity (Temperature T= 2.10+4K) number=2 Normalized intensity in wavelength units, e- and H+ perturbers (Stark only). 10/nm F4 Intensity (Temperature T= 4.10+4K) number=2 Normalized intensity in wavelength units, e- and H+ perturbers (Stark only). 10/nm F8 Intensity (Temperature T= 8.10+4K) number=2 Normalized intensity in wavelength units, e- and H+ perturbers (Stark only). 10/nm F16 Intensity (Temperature T= 16.10+4K) number=2 Normalized intensity in wavelength units, e- and H+ perturbers (Stark only). 10/nm Thomas Schoening, Simona Mei CDS 1995 Jun 08 Schoening T., <uh102ac@usm.uni-muenchen.de> J_A+AS_113_579.xml Interesting lines in the infrared solar spectrum. II: Unblended lines between 1.0 and 1.8um J/A+AS/113/71 J/A+AS/113/71 Lines in the infrared solar spectrum Interesting lines in the infrared solar spectrum. II: Unblended lines between 1.0 and 1.8um J Ramsauer S K Solanki E Biemont Astron. Astrophys. Suppl. Ser. 113 71 1995 1995A&AS..113...71R atomic data line: identification line: profiles Sun: infrared We list 603 spectral lines between 1.0, 1.8um that are judged to be relatively unblended from a visual inspection of spectra of the quiet sun. Much of the atomic data of relevance to studies of solar and stellar magnetism, convection and atmospheric structure are also provided. Particular attention is paid to blending by telluric lines. We determine the level of blending both in the presence and the absence of telluric lines. We also describe how telluric blends may be removed from spectra with high spectral resolution.
Lines judged to be relatively unblended from a visual examination between 1.00 and 1.34um Lines judged to be relatively unblended from a visual examination in the H-band(1.49-1.80um) SolLam Solar wavelength of the lines number=1 Whenever possible {lambda}_sun_ has been determined from the Delbouille et al. (1981) atlas. If the line is too strongly blended in their spectra, then we have obtained the wavelength from the Livingston and Wallace 1991 or Wallace et al. 1993 spectra. All values are only corrected for Doppler shift. 0.1nm Vac Vaccum wavenumber cm-1 n_Vac See number=2 When '*' the wavenumber of this line was taken from a purely solar component of the Livingstone and Wallace (1991) spectral atlas due to the too strong telluric blending of the line in the Delbouille et al. (1981) spectral atlas. --- BlI1 Blending index derived from Delbouille et al. (1981) --- n_BlI1 See number=3 When 'a': In the Delbouille et al. (1981) atlas these lines look less blended than the values given here, but according to the Wallace et al. (1993) and the Livingstone and Wallace (1991) atlases the lines are blended with a telluric line having almost the same wavelength, so that the blends show no readily visible effects. When 'b' line is blended according to Biemont et al. (1985a) --- BlI2 Blending index derived from Livingstone and Wallace (1991) and Wallace et al. (1993) --- Ion Ions and diatomic molecules identified as sources of the solar spectral line --- n_Ion See number=4 When 'a': according to the available log(gf) this identification is extremely unlikely. When 'b' : according to Biemont and Brault (1987a,b) this line is a blend of different hyperfine components --- LabLam Laboratory wavelength of ions, molecules 0.1nm n_LabLam See number=5 When '*' for this line no laboratory wavelength is available in the above references therefore the calculated wavelength has been written instead --- Trans Atomic or molecular transition. The notation of the terms in the identified transitions follows the National Bureau of Standards (NBS) compilations of atomic energy levels, Kurucz (1991) and Nave et al. (1994). --- r_Trans References for transition number=6 For Table1: ---------------------------------- [1] Biemont (1976) [2] Biemont et al. (1985a) [3] Biemont et al. (1985b) [4] Biemont et al. (1986) [5] Biemont et al. (1994) [6] Biemont, Grevesse (1973) [7] Striganov, Sventitskii (1968) [8] Zaidel et al. (1970) [9] Swensson et al. (1970) [10] Kurucz (1991) [11] Kurucz, Peytremann (1975) [12] Livingston, Wallace (1991) [13] Wallace, Livingston (1991) [14] Martin, Zalubas (1983) [15] Reader et al. (1980) [16] Hall (1974) [17] Nave et al. (1994) ----------------------------------- For Table 3: ---------------------------------- [1] Biemont (1976) [2] Biemont et al. (1985a) [3] Biemont et al. (1985b) [4] Biemont et al. (1986) [5] Biemont, Brault (1987a) [6] Biemont, Brault (1987b) [7] Biemont, Grevesse (1973) [8] Hall (1974) [9] Litzen (1976) [10] Litzen, Verges (1976) [11] Johansson, Learner (1990). In accordance with this reference JK notation is used for the levels of the 3d6 4s 6D 4f configuration. [12] Kurucz (1991) [13] Kurucz, Peytremann (1975) [14] Livingston, Wallace (1991) [15] Wallace, Livingston (1991) [16] Martin, Zalubas (1979) [17] Nave, Johansson (1993) [18] Mohler (1955) [19] Nave et al. (1994) --- n_Trans See number=7 When '*' this transition involves a change in orbital angular momentum DL>1, making the identification uncertain. Such identifications are listed only where no other possible identification is known. ! When '!' the order of the multiple line identifications represents their probable contribution to the line (e.g. due to the huge equivalent width of the primary identification, the secondary (blend) probably provides only a very small contribution to the line). a When 'a' this transition involves a change in total spin DS>1 making the identification uncertain. Such identifications are listed only where no other possible identification is known. b When 'b' the sign of the Lande factor of Fe I 15611.151 A is opposite to that expected from the observed Stokes V profile, so that the identification is probably wrong. c When 'c' Ni I 16673.715 A and Ni I 16996.271 A : the laboratory wavelengths of both lines can be matched much better by the calculated wavelengths of the transitions identified by Biemont and Brault (1987b) if the 3d9 5p 1F3o level common to both lies at 48672.085+-0.015 cm-1 (instead of 48671.9 cm-1 listed in Corliss and Sugar, 1981) d When 'd' due to the large equivalent width of the primary identification, the secondary identification (blend) probably contributes only a very minute amount to the line. e When 'e' AlI 16750.614 A is blended with a telluric line of about the same wavelength and is also distorted by the large hyperfine splitting of the given transition (see Biemont and Brault 1987b). --- ExcPot Excitation potential of the lower level of the transition eV gcalc Effective Lande factor calculated from the listed transition --- n_gcalc See number=8 When '*' and 'a' for most transitions the LS coupling Lande factors of the upper and lower levels are used to determine g_eff_. For the levels of the 3d6 4s 6D 4f configuration g values have been taken from Johansson and Learner (1990). When 'a' according to Stokes profile calculations by Muglach and Solanki (1992) the g_eff_ values listed here are incompatible with the observed splittings of these lines. --- gemp Effective Lande factor derived empirically from laboratory measurements --- n_gemp See number=9 If only g_l_ or g_u_ is available from laboratory measurements, the missing atomic level Lande factor is assumed to be represented by its LS coupling value. --- ChiPi Second order coefficient of the {pi}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987) --- ChiSigma Second order coefficient of the {sigma}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987) --- YSigma Third order coefficient of the {sigma}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987) --- CalcLam Calculated wavelength 0.1nm log(gf) Logarithm of the statistically weighted oscillator strength of the corresponding atomic line from Kurucz (1991) --- n_log(gf) See number=10 When 'a' the value was derived from Nave et al. (1994); 'b' from the compilation by Kurucz and Peytremann (1975); 'c' from Biemont et al. (1994); 'd' from Biemont, Grevesse (1973). --- Possible blends rejected as too weak Possible blends rejected as too weak in H-band SolLam Solar wavelength of the lines 0.1nm Ion Ions and diatomic molecules identified as sources of the solar spectral line --- LabLam Laboratory wavelength of ions and molecules 0.1nm n_LabLam See Note (5) in Table 1 and 3 --- ExcPot Excitation potential of the lower level of the transition eV log(gf) Logarithm of the statistically weighted oscillator strength of the corresponding atomic line from Kurucz (1991) --- n_log(gf) See Note (10) in Table 1 and 3 --- table1-2.tex Plain TeX version of table1 and table2 table3-4.tex Plain TeX version of table3 and table4 papdef.tex TeX definitions for tables and paper paper.tex The paper in plain TeX Simona Mei CDS 1995 May 12 J_A+AS_113_71.xml A study of the Chamaeleon star forming region from the ROSAT all-sky survey. I. X-ray observations and optical identifications J/A+AS/114/109 J/A+AS/114/109 Cha X-ray sources & optical identifications A study of the Chamaeleon star forming region from the ROSAT all-sky survey. I. X-ray observations and optical identifications J M Alcala J Krautter J H M M Schmitt E Covino R Wichmann R Mundt Astron. Astrophys. Suppl. Ser. 114 109 1995 1995A&AS..114..109A IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) QSOs X-ray sources ISM: individual (Chamaeleon clouds) stars: pre-main sequence surveys X-rays: stars We present the observations of the ROSAT all-sky survey (RASS) in the direction of the Chamaeleon cloud complex, as well as the spectroscopic identifications of the detected X-ray sources. The main purpose of this identification program was the search for low mass pre-main sequence stars. Sixteen previously known PMS stars were detected with high confidence by ROSAT. Eight are classical T Tauri stars and eight are weak-line T Tauri stars. Seventy-seven new weak-line T Tauri stars were identified on the basis of the presence of strong Li {lambda}6707 absorption, spectral type later than F0 and chromospheric emission. We give coordinates and count rates of the X-ray sources, and present optical spectra and finding charts for the sources identified optically as new pre-main sequence stars. Optical UBV(RI)c and near-infrared JHKLM photometry for this sample of stars is also provided. In addition, 6 new dKe-dMe candidates are found among the RASS sources.
ROSAT
ROSAT all-sky survey X-ray sources in Chamaeleon RXJ RXJ X-ray source name --- m_RXJ Multiplicity index on RXJ --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Count Count rates from ROSAT ct/s e_Count rms uncertainty on Count ct/s ID Optical identification ---- Theta Offset distance arcsec SpType Spectral type --- Type Type number=1 W : previously known weak-line T Tauri star C : previously known classical T Tauri star Wn : new weak-line T Tauri star UAS: unrelated active star UBS: unrelated bright star IR : infrared source QS : quasar RS : radio source G : galaxy. --- Note Appearance in finding chart --- n_Note Note number=2 St.: Stellar, Gal.: galaxy, faint: object fainter than V~20. a : source investigated spectroscopically, but without stellar counterpart found. b : source not investigated. Its corresponding error circle contains objects fainter than our limit for the spectroscopic observations (V~17mag). c : very strong spectroscopic and photometric variability (Alcala et al. 1993A&A...272..225A). d : Halpha filled-in with emission but no Li I A6707 absorption. e : Li I lambda6707 absorption to be confirmed because of low S/N of the spectrum. --- Ref References number=3 1: this Work 2: Simbad catalogue (see ROSAT PSPC, Cat. <IX/11>) 3: Gauvin and Strom (1992ApJ...385..217G) 4: Feigelson and Kriss (1989ApJ...338..262F) 5: Hyland et al. (1982MNRAS.201.1095H) 6: Hughes and Hartigan (1992AJ....104..680H) 7: Walter (1992AJ....104..758W) 8: Feigelson et al. (1993ApJ...416..623F) 9: Huenemoerder et al. (1994MNRAS.271..967H) --- James Marcout, Patricia Bauer CDS 1996 Oct 25 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_114_109.xml Einstein A-coefficients for vibrational transitions in CS J/A+AS/114/175 J/A+AS/114/175 Einstein A-coefficients in CS transitions Einstein A-coefficients for vibrational transitions in CS S Chandra W H Kegel R J Le Roy T Hertenstein Astron. Astrophys. Suppl. Ser. 114 175 1995 1995A&AS..114..175C J/A+AS/117/557 : Einstein A-coefficients for vib-rotational transitions in CO Atomic physics ISM: molecules molecular data stars: abundances Einstein A-coefficients for vib-rotational transitions in CS isotopomers, for vibrational quantum number v up to 20, rotational quantum number J up to 140, and {DELTA}v up to 4, are calculated. The change in J is governed by the selection rules {DELTA}J=+/-1. These coefficients play an important role in astronomy, as CS has been observed in a number of astronomical object.
Einstein A-coefficients, energy of lower level, and frequency of transition for C12S32 Einstein A-coefficients, energy of lower level, and frequency of transition for C12S33 Einstein A-coefficients, energy of lower level, and frequency of transition for C12S34 Einstein A-coefficients, energy of lower level, and frequency of transition for C13S32 Vlow Vibrational quantum number of the lower level --- Jlow Rotational quantum number of the lower level --- Vup Vibrational quantum number of the upper level --- Jup Rotational quantum number of the upper level --- A Einstein A-coefficient s-1 Elow Energy of the lower level of the transition cm-1 Freq Frequency of the transition cm-1 Simona Mei CDS 1995 Jul 26 J_A+AS_114_175.xml CCD photometry of distant open clusters: II NGC 6791 J/A+AS/114/1 J/A+AS/114/1 CCD UBVI photometry of NGC 6791 CCD photometry of distant open clusters: II NGC 6791 J Kaluzny S M Rucinski Astron. Astrophys. Suppl. Ser. 114 1 1995 1995A&AS..114....1K Clusters, open Photometry, CCD Hertzsprung-Russell (HR diagram) novae, cataclysmic variables open clusters and associations: individual (NGC 6791) Three new photometric CCD-based datasets are presented for NGC 6791. They consist of deep UBV photometry (to V_lim_=24, B_lim_=24, U_lim_=23) of the central parts of the cluster and of selected fields around it, and of relatively shallower UBVI photometry for the whole cluster (23'x23'). The data have been used to discuss the reddening, metallicity and age of NGC 6791.
UBV photometry of stars from NGC 6791 field October 91, 2.1-m telescope data UBVI photometry of stars from NGC 6791 field October 92, 0.9-m data ID ID number --- Xpos X coordinate (toward South); 1 pixel=0.68 arcsec pix Ypos Y coordinate (toward West); 1 pixel=0.30 arcsec pix Vmag V magnitude mag e_Vmag rms uncertainty on V magnitude mag o_Vmag Number of averaged V magnitude measurement --- q_Vmag Quality flag for V magnitude number=1 q=1 means relatively poor quality --- B-V B-V colour index mag e_B-V rms uncertainty on B-V number=2 negative sigma means "unknown color" mag o_B-V Number of averaged B measurements --- q_B-V Quality flag for B-V number=1 q=1 means relatively poor quality --- U-B U-B colour index mag e_U-B rms uncertainty on U-B number=2 negative sigma means "unknown color" mag o_U-B Number of averaged U measurements --- q_U-B Quality flag for U-B number=1 q=1 means relatively poor quality --- V-I V-I colour index mag e_V-I rms uncertainty on V-I number=2 negative sigma means "unknown color" mag o_V-I Number of averaged I measurements --- q_V-I Quality flag for V-I --- Simona Mei CDS 1995 Jun 25 J. Kaluzny & S.M. Rucinski <jka@sirius.astrouw.edu.pl> <rucinski@astro.utoronto.ca> J_A+AS_114_1.xml New supernova remnant candidates in M31 J/A+AS/114/215 J/A+AS/114/215 New SNR candidates in M31 New supernova remnant candidates in M31 E A Magnier S Prins J van Paradijs W H G Lewin R Supper G Hasinger W Pietsch J Truemper Astron. Astrophys. Suppl. Ser. 114 215 1995 1995A&AS..114..215M H II regions Supernova remnants galaxies: individual (M 31) galaxies: ISM HII regions ISM: bubbles supernova remnants We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun & Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.
Image parameters Field Field number --- n_Field Note on field number=1 b: images not used in analysis --- RAd Right ascension (J2000.0) deg DEd Declination (J2000.0) deg ExpHa Exposure time in H{alpha} s ExpSII Exposure time in [SII] s ExpV Exposure time in V s NoiseHa Noise/pixel in H{alpha} 10-16mW/m2/pix NoiseSII Noise/pixel in [SII] 10-16mW/m2/pix O and early B stars and their Stroemgren spheres Sp Spectral type --- MVmag Absolute V magnitude mag Vmag Apparent V magnitude mag B-V B-V colour index mag logN(Lyc) Production rate of Lyman continuum photons s-1 logL(Ha) Expected H{alpha} luminosity at the distance of M 31 10-7W logF(Ha) Expected H{alpha} flux at the distance of M 31 mW/m2 U Excitation parameter for such photon rate pc/cm2 Rad Stroemgren sphere radii for a ISM density n_H_=1cm^-3^ pc log(NH) Hydrogen column density for n_H_=1cm^-3^ cm-2 AV Expected optical extinction for n_H_=1cm^-3^ mag Rad100 Stroemgren sphere radii for a ISM density n_H_=100cm^-3^ pc log(NH)100 Hydrogen column density for n_H_=100cm^-3^ cm-2 AV100 Expected optical extinction for n_H_=100cm^-3^ mag Note1 * for HII regions detectable in our images (bold lines in printed table) --- Note2 c for stars included in the completness limit of our blue star list --- The superbubbles Our highest-confidence SNR candidates Our middle-confidence SNR candidates Our lowest-confidence SNR candidates ID Identification number --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg DeltaRA Approximate extent of the object in right ascension arcsec DeltaDE Approximate extent of the object in declination arcsec Diam Diameter of the object arcsec n_Diam When '*' extrapolated diameter --- Pict Picture number --- Fig Figure number (5a through 5m) --- Field Field number in which the candidate was identified --- Comments Comments --- SNR candidates from other authors not identified in our images ID SNR Identification --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Comments Comments --- Simona Mei CDS 1995 Sep 28 J_A+AS_114_215.xml A radio continuum survey of Shapley-Ames Galaxies at 2.8 cm. I. Atlas of radio data J/A+AS/114/21 J/A+AS/114/21 Shapley-Ames Galaxies at 2.8cm A radio continuum survey of Shapley-Ames Galaxies at 2.8 cm. I. Atlas of radio data S Niklas U Klein J Braine R Wielebinski Astron. Astrophys. Suppl. Ser. 114 21 1995 1995A&AS..114...21N VII/51 : Revised Shapley-Ames Catalog of Bright Galaxies (Sandage+, 1981) galaxies: general galaxies: spiral infrared: galaxies radio continuum: galaxies We present measurements of the radio continuum emission at 2.8 cm of a nearly complete sample of spiral galaxies. The sample consists of the Shapley-Ames galaxies north of {delta}=-25deg and brighter than B_T_=+12. The large, nearby galaxies were not observed during the survey, but measured with high sensitivity in individual projects. The radioweak galaxies were also excluded. The observational results and the derived flux densities are given and compared with that of other observations. Pecularities of the radio emission of individual galaxies are discussed.
Results of the 2.8cm survey Name Name of the galaxy (N=NGC) --- RAh Right ascension of optical centre (1950) h RAm Right ascension of optical centre (1950) min RAs Right ascension of optical centre (1950) s DE- Declination sign --- DEd Declination of optical centre (1950) deg DEm Declination of optical centre (1950) arcmin DEs Declination of optical centre (1950) arcsec RAoff =-99 Positional offset of radio source in RA: (RA_radio-RA_opt)*cos(Dec) arcsec DEoff =-99 Positional offset of radio source in declination: (Dec_radio-Dec_opt) arcsec PeakFlux =-001 Peak flux density/beam area mJy S(28cm) Integrated flux density (<0= upper limit) mJy e_S(28cm) Error in integrated flux density mJy log(Lum) Logarithm of monochromatic radio luminosity at 2.8cm W/Hz Reference Reference code number=1 00: own measurements 01: Gioia I.M., Gregorini L., Klein U. =1982A&A...116..164G 02: Klein U., Urbanik M., Beck R., Wielebinski R. =1983A&A...127..177K 03: Urbanik M., Graeve R., Klein U. =1985A&A...152..291U 04: Klein U., Graeve R., Wielebinski R. =1983A&A...117..332K 05: Klein U.., Emerson D.T. =1981A&A....94...25S 06: Krause M., Klein U, Beck R. =1984A&A...138..385K 07: Soida M., Urbanik M., Beck R. =1996A&A..submitted. 08: Neininger N. =1992A&A...263...30N 09: Neininger N., Klein U., Beck R., Wielebinski R. =1991Natur.352..781N 10: Graeve R., Klein U., Wielebinski R. =1990A&A...238...39G 11: Ehle B., Beck R. =1993A&A...273...45E 12: Klein U., Wielebinski R., Morsi H.W. =1988A&A...190...41K 13: Graeve R., Klein U., Wielebinski R. =1981A&A....95..391G 14: Hummel E., Graeve R. =1990A&A...228..315H 15: Israel F.P., van der Hulst J.M. =1983AJ.....88.1736I 16: Garcia-Bareto J.A., Carillo R., Klein U., Dahlem M. 1993, Rev.Mex.Astron.Astrofis., 25, 31 =1993RMxAA..25...31G 17: Niklas S., Klein U., Wielebinski R. =1995A&A...293...56N 18: Dumke M., Krause M., Wielebinski R., Klein U. =1995A&A...302..691D 19: Golla G., 1993, PhD Thesis, University of Bonn 20: Krause M., priv. comm. 21: Urbanik M., priv.comm. --- Simona Mei CDS 1995 May 31 J_A+AS_114_21.xml Linear and non-linear limb-darkening coefficients for the photometric bands R I J H K J/A+AS/114/247 J/A+AS/114/247 Limb-darkening coefficients for R I J H K Linear and non-linear limb-darkening coefficients for the photometric bands R I J H K A Claret J Diaz-Cordoves A Gimenez Astron. Astrophys. Suppl. Ser. 114 247 1995 1995A&AS..114..247C Models, atmosphere Photometry, infrared binaries: eclipsing infrared: general limb-darkening stars: atmospheres We have computed limb-darkening coefficients for five commonly used near infrared photometric bands, namely R, I, J, H, and K, using the stellar atmosphere models by Kurucz (1993). Since the behaviour of the specific intensities is very dependent on the range of effective temperatures considered, we have adopted three analytical approximations to the limb darkening: linear, quadratic and square root. The least-squares method has been adopted for the fit of the limb-darkening coefficients to the model atmospheres.
Linear (u) limb-darkening coefficients logg Surface gravity cm/s+2 Teff Effective temperature K u(R) Linear Limb-darkening coefficient (Filter R) --- u(I) Linear Limb-darkening coefficient (Filter I) --- u(J) Linear Limb-darkening coefficient (Filter J) --- u(H) Linear Limb-darkening coefficient (Filter H) --- u(K) Linear Limb-darkening coefficient (Filter K) --- Quadratic (a, b) limb-darkening coefficients logg Surface gravity cm/s+2 Teff Effective temperature K a(R) Quadratic Limb-darkening coeff. (a) (Filter R) --- b(R) Quadratic Limb-darkening coeff. (b) (Filter R) --- a(I) Quadratic Limb-darkening coeff. (a) (Filter I) --- b(I) Quadratic Limb-darkening coeff. (b) (Filter I) --- a(J) Quadratic Limb-darkening coeff. (a) (Filter J) --- b(J) Quadratic Limb-darkening coeff. (b) (Filter J) --- a(H) Quadratic Limb-darkening coeff. (a) (Filter H) --- b(H) Quadratic Limb-darkening coeff. (b) (Filter H) --- a(K) Quadratic Limb-darkening coeff. (a) (Filter K) --- b(K) Quadratic Limb-darkening coeff. (b) (Filter K) --- Square root (c, d) limb-darkening coefficients logg Surface gravity cm/s+2 Teff Effective temperature K c(R) Square root Limb-darkening coeff. (c) (Filter R) --- d(R) Square root Limb-darkening coeff. (d) (Filter R) --- c(I) Square root Limb-darkening coeff. (c) (Filter I) --- d(I) Square root Limb-darkening coeff. (d) (Filter I) --- c(J) Square root Limb-darkening coeff. (c) (Filter J) --- d(J) Square root Limb-darkening coeff. (d) (Filter J) --- c(H) Square root Limb-darkening coeff. (c) (Filter H) --- d(H) Square root Limb-darkening coeff. (d) (Filter H) --- c(K) Square root Limb-darkening coeff. (c) (Filter K) --- d(K) Square root Limb-darkening coeff. (d) (Filter K) --- Simona Mei CDS 1995 Sep 15 J_A+AS_114_247.xml NGC 7762: a forgotten moderate age open cluster J/A+AS/114/281 J/A+AS/114/281 NGC 7762: a moderate age open cluster NGC 7762: a forgotten moderate age open cluster F Patat G Carraro Astron. Astrophys. Suppl. Ser. 114 281 1995 1995A&AS..114..281P Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 7762) We report CCD B and V photometry for the central region of the old open cluster NGC 7762. The cluster appears very loose and occupies a large sky area. The Colour Magnitude Diagram (CMD) shows a distinct Main Sequence (MS) down to V=~16.5, and a couple of evolved stars. The bottom of the sequence is characterized by a large spread, much greater than the expected broadness due to photometric errors, and probably related to low mass stars evaporation. The analysis here carried out allows us to conclude that NGC 7762 in an intermediate age cluster about 1.8Gyr old. The comparison with theoretical isochrones from the Padova group constrains colour excess and apparent distance modulus in the range 0.85-0.90 and 12.00-12.20, respectively. The distance to the Sun comes out to be 800 pc, somewhat lower than Chincarini's (1966MmSAI..37..423C) estimate.
Photometry ID Star identification number --- C66 Chincarini numbering for common stars --- Xpos X coordinate pix Ypos Y coordinate pix Vmag V magnitude mag B-V B-V colour index mag e_Vmag Error on V magnitude mag Simona Mei CDS 1995 Jul 05 J_A+AS_114_281.xml Multifrequency monitoring of RU Lupi: I. Observations J/A+AS/114/341 J/A+AS/114/341 Multifrequency monitoring of RU Lupi Multifrequency monitoring of RU Lupi: I. Observations F Giovannelli A A Vittone C Rossi L Errico G S Bisnovatyi-Kogan V G Kurt S A Lamzin M Larionov E K Sheffer V N Sidorenkov Astron. Astrophys. Suppl. Ser. 114 341 1995 1995A&AS..114..341G Photometry, UBV Photometry, UBVRI infrared: stars stars: individual (RU Lup) stars: pre-main sequence stars: variables: other ultraviolet: stars X-rays: stars In this paper we present the results of a long campaign of coordinated (sometimes simultaneous) multifrequency observations, from X-ray to radio wavelengths of the extreme T Tauri star RU Lupi. The large amount of data obtained can be useful to understanding the physics governing the intriguing behaviour of this pre-main-sequence star. In particular, from the whole set of data, a model with a protoplanetary accretion disk around a moderately magnetic star seems to be the most promising picture for this source.
RU Lup 15 56 42.2 -37 49 16
UBV photoelectric photometry of RU Lupi in 1983 JD(U) Julian date for observation of U magnitude d Umag U magnitude mag e_Umag rms uncertainty on U mag JD(B) Julian date for observation of B magnitude d Bmag B magnitude mag e_Bmag rms uncertainty on B mag JD(V) Julian date for observation of V magnitude d Vmag V magnitude mag e_Vmag rms uncertainty on V mag UBVRI photoelectric photometry of RU Lupi in 1986 JD(U) Julian date for observation of U magnitude d Umag U magnitude mag e_Umag rms uncertainty on U mag JD(B) Julian date for observation of B magnitude d Bmag B magnitude mag e_Bmag rms uncertainty on B mag JD(V) Julian date for observation of V magnitude d Vmag V magnitude mag e_Vmag rms uncertainty on V mag JD(R) Julian date for observation of R magnitude d Rmag R magnitude mag e_Rmag rms uncertainty on R mag JD(I) Julian date for observation of I magnitude d Imag I magnitude mag e_Imag rms uncertainty on I mag Intensity and equivalent width of emission lines Spect Spectrum number --- Ion Ion --- LamLab Laboratory wavelength 0.1nm EW Equivalent width 0.1nm CrossRef Cross-reference number=1 * Blend with HeI 5876 in low resolution spectra # Blend with H{epsilon} emission line --- Int Continuum intensity in 10-15erg/cm+2/s/0.1nm 10-17W/m2/nm Line/Cont Line to continuum ratio --- Simona Mei CDS 1995 Jul 28 J_A+AS_114_341.xml Coefficients for calculating the second-order moments of the polarization profiles of hydrogen lines J/A+AS/114/363 J/A+AS/114/363 Polarization profiles of H lines Coefficients for calculating the second-order moments of the polarization profiles of hydrogen lines R Casini Astron. Astrophys. Suppl. Ser. 114 363 1995 1995A&AS..114..363C Atomic physics Polarization atomic data atomic processes line: formation polarization In this paper we provide extensive tables of the coefficients that are needed in the calculation of the second-order moments of the polarization profiles of hydrogen lines. We cover all the transitions up to the level n=50, which is enough for many astrophysical applications. We also provide formulae which allow the calculation of the line and oscillator strengths and of the Einstein coefficients for the tabulated transitions.
Coefficients needed in the calculation of the second-order moments of the Stokes profiles of optically-thin, emission hydrogen lines + other related coefficients n First principal quantum number --- m Second principal quantum number --- Omk2(0) Fine-structure contribution to the second-order moment of the intensity profile number=1 Defined in Casini et al. 1994, Eqs. (9) and (10) Ry+2 A0(n,m) First electric coefficient number=2 Defined in Casini et al. 1994, Eq. (14); see also Casini 1995, Eq. (4) --- A2(n,m) Second electric coefficient number=3 Defined in Casini et al. 1994, Eq. (14) --- Om Center-of-gravity frequency of the intensity profile in the absence of external fields number=4 Defined in Casini et al. 1994, Eqs. (12) and (10) Ry Sum Sum of the strengths of the line-components (in units of a0^2, where a0 is the radius of Bohr's first orbit) number=5 Defined in Casini 1995, Eq. (2); a0=h^2^/(4{pi}^2^m_e_ e^2^)=0.5291775x10^-10^m --- Simona Mei CDS 1995 Jul 12 J_A+AS_114_363.xml A ROSAT XUV Pointed Phase Source Catalogue J/A+AS/114/465 J/A+AS/114/465 ROSAT XUV Pointed Phase Source Catalogue A ROSAT XUV Pointed Phase Source Catalogue H C Kreysing H Brunner R Staubert Astron. Astrophys. Suppl. Ser. 114 465 1995 1995A&AS..114..465K IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges et al. 1996) J/ApJS/93/569 : (EUVE) (Bowyer et al. 1994) J/ApJS/96/461 : (FAUST) (Bowyer et al. 1995) J/MNRAS/260/77 : (Pounds et al. 1993) J/MNRAS/274/1165 : (2RE) Pye at al. 1995) Bowyer C., et al., =1994ApJS...93..569B (Catalog <J/ApJS/93/569>) Bowyer C., et al., =1995ApJS...96..461B (Catalog <J/ApJS/96/461>) Brunner H., and Kreysing H.C., 1993, ROSAT/WFC Observer Notes, 93/1 Rev.1 (available by ftp: ait.physik.uni-tuebingen.de, login "xuv", password "xuv_archive"); Pye J.P., et al. =1995MNRAS.274.1165P (Catalog <J/MNRAS/274/1165>) Pounds K.A. et al. =1993MNRAS.260...77P (Catalog <J/MNRAS/260/77>) Voges W., Gruber, R., Haberl, F. et al. 1994, on behalf of the ROSAT Consortium, ROSAT Workshop, MPE, 26 Oct. 1994. X-ray sources catalogs techniques: photometric ultraviolet: stars X-rays: stars We present a catalogue of XUV sources from observations by the Wide Field Camera (WFC) on ROSAT during the pointed phase. The ROSAT WFC is a telescope sensitive in the extreme UV range (17-210eV) which observes in parallel with the ROSAT X-Ray Telescope (XRT). The 5916 pointed observations processed are from the calibration and verification phase in June 1990 and from the period 9 Feb. 1991 to 15 July 1994. The catalogue contains 1022 independent source detections which correspond to 328 individual sources, many of which have been observed repeatedly. Each observation was done with one of four filters S1, S2, P1 and P2. Of the 328 sources 113 are new sources (they are not listed in the "2RE" catalogue) and 274 have been identified with optical counterparts. The catalogue contains coordinates, observed count rates, normalized source count rates and the proposed optical counterpart with its spectral class.
ROSAT
ROSAT XUV Pointed Phase Sources Catalogue ROSAT WFC detections for which no counterpart has been found in other X-ray or UV catalogues RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin Date Date of the beginning of the observation "DD/MM/YY" Dur Effective integration time of observation ks Filter Filter used in the observation number=1 Two different S1 and S2 filters, S1A, S1B, S2A, and S2B, exist. Each filter has a slightly different transmission profile. In most of the observations the S1A and the S2B filter were used, the exceptions are indicated. --- OffAngle Off-axis angle of each source number=2 Count rates for sources with off-axis angles greater than 130' are not reliable. arcmin -ln(Lik) Likelihood of existence --- obsCount Observed source count rate number=3 The observed source count rate and its 1 sigma uncertainty (vignetting corrections applied), as determined by the maximum likelihood fit. ct/ks e_obsCount rms uncertainty on observed source count rate number=3 The observed source count rate and its 1 sigma uncertainty (vignetting corrections applied), as determined by the maximum likelihood fit. ct/ks Count Count rates number=4 Count rates and errors normalized to the detector efficiency at the beginning of the verification phase. ct/ks e_Count Error on count rates number=4 Count rates and errors normalized to the detector efficiency at the beginning of the verification phase. ct/ks Optical Name of the optical counterpart, if identified with objects listed in the SIMBAD data base --- EUV EUV name number=5 As found in the WFC Bright Source Catalogue (Pounds et al. 1993), or from SIMBAD. --- Sp Spectral type number=5 As found in the WFC Bright Source Catalogue (Pounds et al. 1993), or from SIMBAD. --- ROR ROSAT Observation Request number number=6 The ROSAT Observation Request number can be used for retrieving observations from the online in Tuebingen (Brunner and Kreysing 1993). --- Identif Identification of certain types of objects number=7 1: WD, cal, ser; 2: WD, non-cal, ser; 3: WD, cal, target; 4: WD, non-cal, target; 5: not WD, non-cal, target. 'WD' is White Dwarf, 'cal'/'non-cal' means the source was used/not used for the in-flight calibration, 'target'/'ser' means the source was the target of a planned observation or otherwise a serendipitously detected one). --- inEUVE When 'X' the source was found in EUVE (Bowyer et al. 1994) --- in2RE When 'X' the source was found in ROSAT-2RE (Pye et al. 1995) --- inXRT When 'X' the source was found in ROSAT-XRT (Voges et al. 1994) --- inFAUST When 'X' the source was found in FAUST (Bowyer et al. 1995) --- ROSAT WFC sources with average count rates RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin Filter Filter used in the observation; see Note (1) in Table 2 and 5 --- Dur Effective integration time ks Count Count rates; see Note (4) in Table 2 and 5 ct/ks e_Count Error on count rates; see Note(4) in Table 2 and 5 ct/ks Optical Name of the optical counterpart, if identified with objects listed in the SIMBAD data base --- EUV EUV name; see Note (5) in Table 2 and 5 --- Sp Spectral type; see Note (5) in Table 2 and 5 --- inEUVE When 'X' the source was found in EUVE (Bowyer et al. 1994) --- in2RE When 'X' the source was found in ROSAT-2RE (Pye et al. 1995) --- inXRT When 'X' the source was found in ROSAT-XRT (Voges et al. 1994) --- inFAUST When 'X' the source was found in FAUST (Bowyer et al. 1995) --- Simona Mei CDS 1995 Jun 27 J_A+AS_114_465.xml Photographic observations of visual double stars J/A+AS/114/487 J/A+AS/114/487 Photographic observations of visual binaries Photographic observations of visual double stars D M D Jasinta M Raharto E Soegiartini Astron. Astrophys. Suppl. Ser. 114 487 1995 1995A&AS..114..487J I/196 : HIC Catalogue (Turon et al., 1993) I/211 : CCDM Catalogue (Dommanget and Nys, 1994) J/A+AS/107/235 : Observations of binaries (Jasinta & Soegiartini, 1994) Jasinta D.M.D., Soegiartini E. =1994A&AS..107..235J Turon C., et al., 1992, The Hipparcos Input Catalogue, ESA-The INCA Consortium van Albada-van Dien E. =1983A&AS...52..193V Stars, double and multiple astrometry binaries: visual We present the results of photographic observations of 399 visual double stars of the Hipparcos Input Catalogue (HIC), observed in the years 1980 and 1990-1991 with the 60-cm double-refractor of the Bosscha Observatory at Lembang, Java.
Photographic observations of visual double stars CCDM CCDM number number=1 Catalogue of the components of double and multiple stars; Dommanget 1994, Comm. Obs. R. Belgique, Ser. A, N. 115 Catalogue <I/211> --- Comp Components --- RAh Right Ascension (2000) h RAm Right Ascension (2000) min RAs Right Ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Star Star name --- Mag1 First component magnitude mag n_Mag1 Separation sign --- Mag2 Second component magnitude mag Spect Spectra of the components --- Epoch Mean epoch of observations yr SepRA Mean value of D{alpha}cos{delta} arcsec e_SepRA Standard error on D{alpha}cos{delta} mas SepDE Mean value of D{delta} arcsec e_SepDE Standard error on D{delta} mas Rho Angular distance arcsec e_Rho Standard error in angular distance mas Theta Position angle deg e_Theta Standard error in position angle 10-2deg Plates Number of plates --- Images Number of images --- Weight Weight --- Simona Mei CDS 1995 Jul 28 J_A+AS_114_487.xml UBVRI-CCD photometry of Cepheus OB3 association J/A+AS/114/489 J/A+AS/114/489 UBVRI CCD photometry of Cepheus OB3 UBVRI-CCD photometry of Cepheus OB3 association C Jordi D Galadi-Enriquez E Trullols F Lahulla Astron. Astrophys. Suppl. Ser. 114 489 1995 1995A&AS..114..489J instrumentation: detectors open clusters and associations: individual (Cep OB3) stars: general techniques: photometric Johnson CCD photometry was performed in the two subgroups of the association Cepheus OB3, for selected fields each containing at least one star with previous UBV photoelectric photometry. Photometry for about 1000 stars down to visual magnitude 21 is provided, although the completeness tests show that the sample is complete down to V=19mag. Individual errors were assigned to the magnitude and colours for each star. Colour-colour and colour-magnitude diagrams are shown. Astrometric positions of the stars are also given. Description of the reduction procedure is fully detailed.
UBVRI photometry Star Star identification --- Xpos X position pix Ypos Y position pix RAh Right ascension J2000.0 h RAm Right ascension J2000.0 min RAs Right ascension J2000.0 s DE- Declination sign --- DEd Declination J2000.0 deg DEm Declination J2000.0 arcmin DEs Declination J2000.0 arcsec Vmag V magnitude mag e_Vmag Error on V magnitude mag B-V B-V colour index mag e_B-V Error on B-V mag U-B U-B colour index mag e_U-B Error on U-B mag V-R V-R colour index mag e_V-R Error on V-R mag V-I V-I colour index mag e_V-I Error on V-I mag n_Star Notes number=1 a: Stars cross-identified with other catalogues: Star BHJ GSC PPM BD SAO HD HIC --------- ---- --------- ----- -------- ----- ------ ----- BHJ11-017 11 428200996 24019 +61 2357 20289 BHJ15-019 15ft BHJ20-012 17ft 428200959 BHJ20-016 17br 428200930 BHJ20-056 20 428200941 24036 +61 2364 20305 216711 113065 BHJ20-086 428200454 BHJ23-039 428200339 BHJ23-042 428200701 BHJ23-067 23 428200989 BHJ24-044 24 428200710 24049 +61 2366 20316 BHJ24-052 428200429 BHJ25-052 25 428200544 BHJ27-035 428200695 BHJ27-048 27 428200501 BHJ27-051 428200456 BHJ28-078 28 428200488 BHJ30-014 428200393 BHJ30-034 30 428200795 24057 +61 2369 20322 BHJ34-011 428200319 BHJ34-019 33ft 428200563 BHJ34-020 33br 428200551 BHJ40-111 40 428200933 24072 +61 2372 20334 217061 113301 BHJ40-130 428200556 BHJ43-009 428200895 BHJ43-011 43 428200844 24083 +61 2374 20341 217174 BHJ44-038 428200293 BHJ44-089 44br 428200415 24088 +62 2142 20346 BHJ44-093 44ft 428200704 BHJ54-016 54 428200548 24108 +62 2152 20358 217463 113538 BHJ64-022 428200390 24121 +61 2381 20366 BHJ64-031 64 428200659 24124 +61 2382 20370 113680 BHJ65-022 65 +62 2158 BHJ70-031 428201038 BHJ70-041 428201017 BHJ70-081 428200778 BHJ70-086 70 428200449 24169 +62 2166 20406 BHJ80-006 80 428200072 24211 +61 2396 20440 114225 ---------------------------------------------------------------------- b: The positions for the stars in this field were calculated taking as origin BHJ15br (PPM24029, BD+61 2361, SAO20299, HD216629, HIC113017). Its frame coordinates are x=289.059 y=479.793, and the J2000 equatorial coordinates taken from PPM catalogue alpha=22h53m15.63s, delta=+62deg 08' 44.76". It was not obtained V magnitude for BHJ15br and, thus, we can not give photometry for this star. c: The only positional information found for stars in this field comes from the cross-identification BHJ65 = BD+62 2158 (alpha(B1950)=23h 00.1m, delta(B1950)=+62deg33'). The resulting absolute positions accuracy is, so, not better than 1'. --- Simona Mei CDS 1995 Jul 07 J_A+AS_114_489.xml P Cygni - spectral atlas with complete line identifications in the wavelength range from 4840 to 6760 A J/A+AS/114/499 J/A+AS/114/499 Spectral Atlas of P Cygni in range 4840-6760A P Cygni - spectral atlas with complete line identifications in the wavelength range from 4840 to 6760 A N Markova R Zamanov Astron. Astrophys. Suppl. Ser. 114 499 1995 1995A&AS..114..499M Spectroscopy atlases line: identification stars: individual (P Cyg) Using the coude spectrograph of the NAO 2m RCC telescope at the Rhodope Mountains, Bulgaria, 11 spectra in the wavelength range from 4840 to 6760A of P Cygni were obtained during the years 1981, 1983 and 1985. By averaging these spectra we achieved a S/N-ratio of about 50. Here we present a spectral atlas with complete line identifications. Apart from the lines listed by de Groot (1969) many pure bright lines are identified. Most of them are lines of FeIII with high multiplet numbers and NII. Further emission lines are those of SiII multiplets 2, 4 and 5. A new feature is SII spectrum in absorption and emission. In addition to the forbidden lines discovered by Stahl et al. (1991, 1993) three new lines, [FeII19] {lambda}5159, [FeII18] {lambda}5273 and [FeII34] {lambda}5477 are identified. The presence of some [TiII9] lines as well as the red lines of [NII1] is considered as quite probable.
P Cyg HR 7763 HD 193237 20 17 47.1 +38 01 59
P Cygni spectrum - wavelengths and identifications LamObs Observational wavelengths 0.1nm n_LamObs When "?" It's an uncertain feature --- Nat Nature of the line number=1 a= absorption e= emission --- n_Nat When ')': This feature and the following are believed to be formed by the same line or lines --- LamLab Laboratory wavelengths 0.1nm n_LamLab Uncertainty sign --- Ion Identification element --- n_Ion '*' marks the most important contributor to a blend --- Remarks Remarks number=2 new= newly identified line 1= line observed by de Groot (1969) 2= line observed by Stahl et al. (1993) --- Remarks2 Additional remarks number=3 IS= interstellar line bl= blend --- n_ForbidLine "--" marks the area of overlapping of forbidden and permitted line --- ForbidLine Forbidden line identification --- n2_ForbitLine ? = an uncertain identification --- Simona Mei CDS 1995 Jul 25 J_A+AS_114_499.xml The UV properties of normal galaxies. III Standard Luminosity Profiles and Total Magnitudes J/A+AS/114/527 J/A+AS/114/527 UV properties of normal galaxies. III. The UV properties of normal galaxies. III Standard Luminosity Profiles and Total Magnitudes A Rifatto G Longo M Capaccioli Astron. Astrophys. Suppl. Ser. 114 527 1995 1995A&AS..114..527R J/A+AS/109/341 : Paper II Galaxies, photometry Photometry, ultraviolet catalogs galaxies: photometry ultraviolet: galaxies In the previous papers of this series (Longo et al. =1991A&AS...90..375L; Rifatto et al. =1995A&AS..109..341R) we collected and reduced to the same system all the available photometric data obtained in the ultraviolet (UV) range for normal (i.e. non active) galaxies. Here we use these data to derive standard UV luminosity profiles for three morphological bins (E/S0; Sa/Sb; Sc/Sd) and extrapolated total magnitudes for almost 400 galaxies. We find that: 1) the UV growth curves are well matched by the B-band revised standard luminosity profiles, once a proper shift in the effective radius is applied, and 2) the UV light in early-type galaxies is more centrally concentrated than the visible light.
List of normal galaxies with UV total mag. Id Identification --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec MType Morphological type --- Log(Ae) Dec. log of the effective aperture 0.1arcmin l_UV1mag Limit flag on UV1 magnitude --- UV1mag UV1 magnitude (1650 A) mag e_UV1mag Error on UV1 magnitude mag n_UV1mag See Note number=1 G: the magnitude was extrapolated from GUV S: the magnitude was extrapolated from SCAP A: the magnitude was extrapolated from ASTROBEE *: the magnitude can be overestimated due to the contribution from overlapping nearby galaxies unresolved by the GUV beam --- l_UV2mag Limit flag on UV2 magnitude --- UV2mag UV2 magnitude (2500 A) mag e_UV2mag Error on UV2 magnitude mag n_UV2mag See Note number=1 G: the magnitude was extrapolated from GUV S: the magnitude was extrapolated from SCAP A: the magnitude was extrapolated from ASTROBEE *: the magnitude can be overestimated due to the contribution from overlapping nearby galaxies unresolved by the GUV beam --- UV3mag UV3 magnitude (3150 A) mag e_UV3mag Error on UV3 magnitude mag Simona Mei CDS 1995 Jul 28 J_A+AS_114_527.xml A deep BVI photometric study of the open cluster NGC 2453 J/A+AS/114/537 J/A+AS/114/537 BVI photometric study of NGC 2453 A deep BVI photometric study of the open cluster NGC 2453 D C V Mallik R Sagar A K Pati Astron. Astrophys. Suppl. Ser. 114 537 1995 1995A&AS..114..537M Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 2453) planetary nebulae: individual (NGC 2452) stars: evolution CCD observations of the open cluster NGC 2453 have been carried out in B, V and I passbands. A total of 356 stars have been observed in a field of about 4'x6' of the sky centred on the cluster. Colour-magnitude diagrams in V, B-V and V, V-I have been generated down to V=20 and for the first time, the unevolved part of the cluster main sequence has been observed. The mean true distance modulus derived from these diagrams is 13.mag 85+/-0.2 yielding a distance of 5.9+/-0.2kpc. A mean age of 25Myr has been derived for the cluster by fitting isochrones. The distance of approximately 6kpc puts the cluster much beyond the planetary nebula NGC 2452 whose largest estimated distance to date is about 3.5kpc. The two are not physically associated.
NGC 2453 C 0745-271 07 47.8 -27 14
BVI photometry of 356 stars in the Region of NGC 2453 Star Star number --- Xpos X coordinate pix Ypos Y coordinate pix Vmag V magnitude mag B-V B-V colour index mag V-I V-I colour index mag CrossId Cross identification of stars number=1 G: Gathier 1984 MF: Moffat and Fitzgerald 1974 S: Seggewiss 1971 --- Simona Mei CDS 1995 Jul 26 J_A+AS_114_537.xml Stellar models for a wide range of initial chemical compositions until helium burning. II. From X=0.63 to X=0.80, for Z=0.01. J/A+AS/114/549 J/A+AS/114/549 Stellar models until He burning - II. Stellar models for a wide range of initial chemical compositions until helium burning. II. From X=0.63 to X=0.80, for Z=0.01. A Claret A Gimenez Astron. Astrophys. Suppl. Ser. 114 549 1995 1995A&AS..114..549C J/A+AS/109/441 : Paper I (From X=0.60 to X=0.80 for Z=0.02) Models, evolutionary binaries: general stars: abundances stars: evolution stars: fundamental parameters stars: interiors Three new grids of stellar evolutionary models with Z=0.01 are presented for the following values of initial hydrogen content X_i_=0.80, 0.73 and 0.63. The latest set of radiative opacities with spin-orbit coupling provided by the Lawrence Livermore group are used. For the lower temperatures the results by Alexander were considered. The models were computed taking into account core overshooting and mass loss. The grids cover the mass range between 1 and 40M_{sun}_. The internal structure constants (k_j_,j=2, 3,4) and the moment of inertia are also computed. These parameters are needed to investigate apsidal motions and tidal interactions in double-lined eclipsing binaries. This paper is part of a project which aims to provide grids of stellar models for a wide range of metal and hydrogen content.
All models with Z=0.01, X=0.80, 0.73 and 0.63 logM Initial mass of the model solMass X X initial composition (H) --- Z Z initial composition --- Overshoot without (0) or with (1) overshooting --- Age Age of models yr log(L) Total luminosity solLum log(g) Surface gravity cm/s2 log(Teff) Effective temperature K log(k2) Apsidal motion constant (j=2) --- log(k3) Apsidal motion constant (j=3) --- log(k4) Apsidal motion constant (j=4) --- alpha alpha = -E_p x R/GM^2 --- beta Fractional gyration radius ---- Simona Mei CDS 1995 Oct 18 UNKNOWN UNKNOWN * 18-Oct-1995: received at CDS from Antonio Claret dos Santos <aclaret@ll.iac.es> * 23-Jan-1996: tables converted to a format identical to Paper I J_A+AS_114_549.xml New measurement of radial velocities in clusters of galaxies. IV. J/A+AS/114/565 J/A+AS/114/565 Radial velocities in clusters of galaxies. New measurement of radial velocities in clusters of galaxies. IV. D Proust A Mazure C Vanderriest L Sodre Jr. H V Capelato Astron. Astrophys. Suppl. Ser. 114 565 1995 1995A&AS..114..565P galaxies: clusters: general galaxies: distances and redshifts We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.
Heliocentric redshifts for galaxies Cluster Abell cluster name --- No Galaxy number --- Name IC or MCG name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Mtype Morphological type from Dressler's (1980) --- Vmag Estimated total apparent visual magnitude (Dressler, 1980) mag HRV Heliocentric radial velocity km/s e_HRV rms uncertainty on HRV km/s Inst Intrumentation number=1 e: 1.50m ESO telescope o: 1.93m OHP telescope + CARELEC spectrograph s: 1.93m OHP telescope + SILFID spectrograph --- Notes Notes number=2 1: H{beta} = 16106 km/s; H{alpha} = 16046 km/s 2: H{alpha} = 9355 km/s 3: OII = 18710 km/s 4: H{beta} = 11919 km/s, H{alpha} = 11939 km/s --- Galaxies observed through the galactic plane at OHP Name Galaxy name --- MCG MCG name (catalogue <VII/100>) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Mtype Type --- Vmag Total apparent visual magnitude mag Diam Diameter mag e_Diam rms uncertainty on diameter mag HVR Heliocentric radial velocity km/s e_HVR rms uncertainty on HVR km/s Note Note 1: emission lines are H{gamma}, H{beta}, 2*OIII --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Jan 15 J_A+AS_114_565.xml Linear polarimetry of Ap stars. V. A general catalogue of measurements J/A+AS/114/79 J/A+AS/114/79 Polarimetry of Ap stars: general catalogue Linear polarimetry of Ap stars. V. A general catalogue of measurements J L Leroy Astron. Astrophys. Suppl. Ser. 114 79 1995 1995A&AS..114...79L catalogs polarization stars: chemically peculiar stars: magnetic fields A systematic program of broadband linear polarimetry, bearing on 55 Ap stars, has been developed during the 4 last years, at the Pic du Midi Observatory. While separate data have been already published, we present in this paper a complete catalogue of our observational material, including more than 400 measurements. We complement these data with another 100 measurements, obtained previously by other authors, so as to get a synthetic view of the phenomenon. Most of the observations have been dedicated to a small number (15) of stars, which show conspicuous changes of the linear polarization, so that it is possible to know accurately the time variation of the Stokes parameters: we expect that these new data will really improve our knowledge of the magnetic configuration, after a proper analysis which is currently being developed. For the other 40 stars, the polarization is either too small, or strongly contaminated by the interstellar polarization, so that broadband polarimetry is not very effective. Anyway, this first systematic investigation on the linear polarization of Ap stars will be a useful starting point for future measurements which should be made with higher spectral resolution. Finally, our measurements have provided new determinations of the rotation period for several stars.
Polarization data (polariz.dat 1 to 68) Star Star name number=1 HD 11502 = {gamma} Ari S HD 11503 = {gamma} Ari N --- Filter Filter number=2 B : B filter Ba : B filter; Piirola and Tuominen 1981 Bb : B filter; Breger et al. 1989 Bc : B filter; Berdyugin et al. 1992 exB : extended-B filter; Kemp and Wolstencroft 1974 L : {lambda}=4200A filter L5 : {lambda}=5200A filter LB : {lambda}=4200A or B filter --- JD Julian Date d Pol Polarization degree % Theta Polarization orientation deg Q/I Reduced Stokes parameter Q/I % U/I Reduced Stokes parameter U/I % e_Q/I Standard deviation on Q/I and U/I % Fourier coefficients of the Q/I and U/I expansion Star Star name --- ZQ Fourier coefficient Z_Q_ --- AQ Fourier coefficient A_Q_ --- BQ Fourier coefficient B_Q_ --- CQ Fourier coefficient C_Q_ --- DQ Fourier coefficient D_Q_ --- EQ Fourier coefficient E_Q_ --- FQ Fourier coefficient F_Q_ --- GQ Fourier coefficient G_Q_ --- HQ Fourier coefficient H_Q_ --- IQ Fourier coefficient I_Q_ --- JQ Fourier coefficient J_Q_ --- ZU Fourier coefficient Z_U_ --- AU Fourier coefficient A_U_ --- BU Fourier coefficient B_U_ --- CU Fourier coefficient C_U_ --- DU Fourier coefficient D_U_ --- EU Fourier coefficient E_U_ --- FU Fourier coefficient F_U_ --- GU Fourier coefficient G_U_ --- HU Fourier coefficient H_U_ --- IU Fourier coefficient I_U_ --- JU Fourier coefficient J_U_ --- Chi2/nu Ratio of Chi-squared to the number of degrees of freedom --- Simona Mei CDS 1995 Jul 05 J_A+AS_114_79.xml Optical identifications of radio sources from the 1 Jy, S4 and S5 catalogues J/A+AS/115/11 J/A+AS/115/11 Optical identifications of radio sources Optical identifications of radio sources from the 1 Jy, S4 and S5 catalogues M Stickel H Kuehr Astron. Astrophys. Suppl. Ser. 115 11 1996 1996A&AS..115...11S III/175 : (gathers papers I-V) J/A+AS/80/103 : (I) J/A+AS/97/483 : (II) J/A+AS/98/393 : (II-Observational data) J/A+AS/100/395 : (III) J/A+AS/101/521 : (IV) J/A+AS/103/349 : (Update of optical identifications) J/A+AS/105/67 : (Optical identifications from 1Jy, S4, S5) J/A+AS/105/211 : (Optical identification of 1Jy) Ekers R.D. et al. 1989, MNRAS 236, 737 =1989MNRAS.236..737E Fey A.L. et al. 1992, AJ 104, 891 =1992AJ....104..891F Fey A.L. et al. 1994, AJ 107, 385 =1994AJ....107..385F Kapahi V.K. 1981, A&AS 43, 381 =1981A&AS...43..381K Kuehr H. et al. 1981, A&AS 45, 367 =1981A&AS...45..367K Kuehr H. et al. 1987, A&AS 71, 493 =1987A&AS...71..493K Morabito D.D. et al. 1982, AJ 87, 517 =1982AJ.....87..517M Morabito D.D. et al. 1983, AJ 88, 1138 =1982AJ.....87..517M Morabito D.D. et al. 1985, AJ 90, 590 =1985AJ.....90..590M Morabito D.D. et al. 1986, AJ 92, 546 =1986AJ.....92..546M Morganti D.D. et al. 1993, MNRAS 263, 1023 =1993MNRAS.263.1023M Patnaik A.R. et al. 1992, MNRAS 254, 655 =1992MNRAS.254..655P Pauliny-Toth I.I.K. et al. 1978, AJ 83, 451 =1978AJ.....83..451P Pearson T.J. and Readhead A.C.S. 1988, ApJ 328, 114 =1988ApJ...328..114P Perley R.A. 1982, AJ 87, 859 =1982AJ.....87..859P Robertson D.S. et al. 1993, AJ 105, 353 =1993AJ....105..353R Russell J.L. et al. 1994, AJ 107, 379 =1994AJ....107..379R Ulvestad J. et al. 1981, AJ 86, 1010 =1981AJ.....86.1010U Vigotti M. et al. 1989, AJ 98, 419 =1989AJ.....98..419V White G.L. 1992, Proc. Astron. Soc. Australia 10,140 =1992PASAu..10..140W Active gal. nuclei QSOs Radio sources Redshifts catalogs galaxies: active quasars: general radio continuum: general surveys CCD images of the fields of 115 radio sources from the 1Jy, S4 and S5 catalogues are presented. New optical counterparts have been found for a total of 34 sources, a large fraction of which had as yet only been described as empty fields on Sky Survey Plates. Of the 54 radio sources with previously published identifications, 50 optical counterparts have been confirmed while for 4 sources new identifications are proposed. R band magnitudes, derived from the CCD images, are provided for all but a few identified optical counterparts. The fields at the positions of 27 radio sources are still empty down to a limiting magnitude of at least m_R_=22mag, requiring much deeper optical as well as additional infrared images for establishing their optical counterparts.
Observed 1 Jy Radio Sources Observed S4 Radio Sources Observed S5 Radio Sources Name Source name --- RAh Right ascension of the radio source (1950) h RAm Right ascension of the radio source (1950) min RAs Right ascension of the radio source (1950) s DE- Declination sign --- DEd Declination of the radio source (1950) deg DEm Declination of the radio source (1950) arcmin DEs Declination of the radio source (1950) arcsec RefPos Reference to the radio position number=1 AC White (1992) BV Vigotti et al. (1989) D Pearson and Readhead (1988) EK Ekers et al. (1989) FY1 Fey et al. (1992) FY2 Fey et al. (1994) J Kuehr et al. (1981) K Kapahi (1981) M1 Morabito et al. (1982) M2 Morabito et al. (1983) M3 Morabito et al. (1985) M4 Morabito et al. (1986) MK Morganti et al. (1993) P Perley (1982) PA Patnaik et al. (1992) RO Robertson et al. (1993) RU2 Russell et al. (1994) S4 Pauliny-Toth et al. (1978) S5 Kuehr et al. (1987) U Ulvestad et al. (1981) VLA VLA Calibrator position --- Bright Brightness of the optical counterpart mag SouType Source type --- z Redshift --- S5GHz Radio flux density S_5GHz_ Jy SpIndex Radio spectral index between 11 cm and 6 cm --- Journal of 1 Jy Observations Journal of S4 Observations Journal of S5 Observations Name Source name --- Date Date of observation --- Telescope Telescope used for the observation --- Time Total integration time s Seeing Estimate of the seeing during the observation arcsec Scale Scale of the CCD image arcsec/pix Simona Mei CDS 1995 Sep 06 J_A+AS_115_11.xml The current optical identification status of the S5 radio source catalogue J/A+AS/115/1 J/A+AS/115/1 Optical identification of S5 catalog The current optical identification status of the S5 radio source catalogue M Stickel H Kuehr Astron. Astrophys. Suppl. Ser. 115 1 1996 1996A&AS..115....1S III/175 : (gathers papers I-V) J/A+AS/80/103 : (I) J/A+AS/97/483 : (II) J/A+AS/98/393 : (II-Observational data) J/A+AS/100/395 : (III) J/A+AS/101/521 : (IV) J/A+AS/103/349 : (Update of optical identifications) J/A+AS/105/67 : (Optical identifications from 1Jy, S4, S5) J/A+AS/105/211 : (Optical identification of 1Jy) J/A+AS/115/11 : (Optical identification of 1Jy, S4, S5) Burbidge G., Crowne A.H., 1979, ApJS 40,583 =1979ApJS...40..583B Condon J.J., Broderick J.J., 1988, AJ 96, 30 =1988AJ.....96...30C Djorgovski S., Spinrad H., McCarthy P., Dickinson M., V; Breugel W., Strom R.G., 1988, AJ 96,836 =1988AJ.....96..836D Dunlop J.S., Peacock J.A., Savage A., Lilly S.J., Heasly J.N., Simon A.J.B., 1989, MNRAS 238, 1171 =1989MNRAS.238.1171D Eckart A., Witzel A., Biermann P., Johnston K.J., Simon E, Schalinski C., Kuhr H., 1986, A&A 168,17 =1986A&A...168...17E Fey A.L., Russell J.L., Ma C., et al., 1992, AJ 104,891 =1992AJ....104..891F Fey A.L., Russell J.L., de Vegt C., et al., 1994, AJ 107, 385 =1994AJ....107..385F Herbig T., Readhead A.C.S., 1992, ApJS 81, 83 =1992ApJS...81...83H Hewitt A., Burbidge G., 1991, ApJS 75, 297 =1991ApJS...75..297H Hewitt A., Burbidge G., 1993, ApJS 87, 451 =1993ApJS...87..451H Kristian J., Sandage A., Katem B., 1978, ApJ 219, 803 Kuhr H., 1980, PhD Thesis, University of Bonn, Germany Kuhr H., Witzel A., Pauliny-Toth I.I.K., Nauber U., 1981a, A&AS 45, 367 Kuhr H., Pauliny-Toth I.I.K., Witzel A., Schmidt J., 1981b, AJ 86, 854 Kuhr H., Johnston K.J., Odenwald S., Adlhoch J., 1987, A&AS 71, 493 Kuhr H., Schmidt G.D., 1990, AJ 99, 1 McCarthy P., 1988, PhD Thesis, University of California, Berkeley Lawrence C.R., Pearson T.J., Readhead A.C.S., Unwin S.C., 1986, AJ 91, 494 =1986AJ.....91..494L O'Dea C.P., Baum S.A., Stanghellini C., 1991, ApJ 380, 66 =1991ApJ...380...66O O'Dea C.P., Davies J.K., Stanghellini C., Baum S.A., Laurikainen E., 1992, Preliminary results of optical and near infrared imaging of GPS radiosources: Evidence for an obscured AGN? In: Holt S., Neff S.G., Urry C.M. (eds.) Testing the AGN Paradigm. AIP Conf. Proc. 254, New York, p. 435 Patnaik A.R., Browne I.W.A., Wilkinson, P.N., Wrobel J.M., 1992, MNRAS 254, 655 =1992MNRAS.254..655P Pauliny-Toth I.I.K., Witzel A., Preuss E., Kuhr H., Kellermann K.I., Fomalont E.B., Davies M.M., 1978, AJ 83, 451 =1978AJ.....83..451P Peacock J.A., Perryman M.A.C., Longair M.S., Gunn J.E., Westphal J.A., 1981, MNRAS 194, 601 Poladitis A.G., Wilkinson P.N., Xu W., Readhead A.C.S., Pearson T.J., Taylor G.B., Vermeulen R.C., 1995 (preprint) Riley J.M., 1989, MNRAS 238, 1055 =1989MNRAS.238.1055R Robertson D.S., Carter W.E., Ray J.R., Dillinger W.H., et al., 1993, AJ 105, 353 =1993AJ....105..353R Russell J.L., Jauncey D.L., Harvey B.R., et al., 1992, AJ 103, 2090 =1992AJ....103.2090R Smith H.E., Burbidge E.M., Spinrad H., 1976, ApJ 210, 627 Sovers O.J., Edwards C.D., Jacobs C.S., Lanyi G.E., Liewer K.M., Treuhaft R.N., 1988, AJ 95, 1647 =1988AJ.....95.1647S Spinrad H., Djorgovski S., Marr J., Aguilar L., 1985, PASP 97, 932 =1985PASP...97..932S Stanghellini C., O'Dea C.P., Baum S.A., Laurikainen E., 1993, ApJS 88, 1 =1993ApJS...88....1S Stickel M., Kuhr H., Fried J.W., 1993a, A&AS 97, 483 =1993A&AS...97..483S Stickel M., Fried J.W., Kuhr H., 1993b, A&AS 98, 393 =1993A&AS.. 98..393S Stickel M., Kuhr H., 1993a, A&AS 100, 395 =1993A&AS..100..395S Stickel M., Kuhr H., 1993b, A&AS 101, 521 =1993A&AS..101..521S Stickel M., Kuhr H., 1994a, A&AS 103, 349 =1994A&AS..103..349S Stickel M., Kuhr H., 1994b, A&AS 105, 67 =1994A&AS..105...67S Stickel M., Meisenheimer K., Kuhr H., 1994, A&AS 105, 211 =1994A&AS..105..211S Stickel M., Kuhr H., 1995, A&AS (in press) Taylor G.B., Vermeulen R.C., Pearson T.J., et al., 1994, ApJS 95, 345 =1994ApJS...95..345T Vermeulen R.C., Taylor G.B., 1995, AJ 109, 1983 Veron-Cetty M.P., Veron P., 1983, A&AS 53, 219 =1983A&AS...53..219V Veron-Cetty M.P., Veron P., 1993, ESO Scientific Report No. 13 Wall J.V., Peacock J.A., 1985, MNRAS 216, 173 =1985MNRAS.216..173W Waltman E., Johnston K.J., Spencer J.H., Pauliny-Toth I., Schraml J., Witzel A., 1981, A&A 101, 49 Xu W., Lawrence C.R., Readhead A.C.S., Pearson T.J., 1994, AJ 108, 395 =1994AJ....108..395X Active gal. nuclei QSOs Radio sources catalogs galaxies: active quasars: general radio continuum: galaxies radio continuum: general surveys Optical identifications, magnitudes, and redshifts have been compiled for the 185 radio sources of the S5 catalogue, representing its current optical identification status. Reliable optical counterparts are found for more than 75% of the sources, nearly 50% of which have measured redshifts. Our tabulation also includes radio positions, radio fluxes, and radio spectral indices. References to other catalogues and detailed supplementary notes are given for a large fraction of the sources.
The S5 radio source catalogue Seq Sequence number --- Name Radiosource name --- RAh Right ascension 1950, radioposition h RAm Right ascension 1950, radioposition min RAs Right ascension 1950, radioposition s DE- Declination sign --- DEd Declination 1950, radioposition deg DEm Declination 1950, radioposition arcmin DEs Declination 1950, radioposition arcsec RefPos References to the radio position number=1 A Waltman et al. (1981) B Hewitt & Burbidge (1993) Be Hewitt & Burbidge (1991) C Spinrad et al. (1985) FY1 Fey et al. (1992) FY2 Fey & al. (1994) G Burbidge & Crowne (1979) J Kuehr et al. (1981a), Stickel et al. (1994) PA Patnaik et al. (1992) R Veron-Cetty & Veron (1983) RO Robertson et al. (1993) RU Russell et al. (1992) S4 Pauliny-Toth et al. (1978) S5 Kuehr et al. (1987) SO Sovers et al. (1988) V Veron-Cetty & Veron (1993) VLA VLA Calibrator position --- Bright Brightness of the optical counterpart mag Id Optical counterpart identification (? indicates uncertainty entry) --- z Optical counterpart redshift --- S5GHz Radio flux density at 5 GHz Jy SpIndex Radio spectral index between 11cm and 6cm --- Ref References, see file notes --- Notes to table1 Name Radiosource name --- Text Text of note; references are explained below --- Patricia Bauer CDS 1996 Feb 27 J_A+AS_115_1.xml Photometric Bgr survey of the distant clusters of galaxies Cl 1613+3104 and Cl 1600+4109 J/A+AS/115/219 J/A+AS/115/219 Bgr survey of Cl1613+3104 and Cl1600+4109 Photometric Bgr survey of the distant clusters of galaxies Cl 1613+3104 and Cl 1600+4109 R Pello R Vilchez-Gomez Astron. Astrophys. Suppl. Ser. 115 219 1996 1996A&AS..115..219P Clusters, galaxy Photometry, CCD galaxies: clusters: individual (Cl 1613+3104, CI 1600+4109) A set of photometric data concerning two distant clusters of galaxies is presented : Cl1613+3104 (z=0.415) and Cl1600+4109 (z=0.540). The photometric survey extends to a field of about 4x3 arcmin. It was performed in 3 filters: Johnson B, and Thuan-Gunn g and r. The sample includes 679 objects in the field of Cl1613+3104 and 335 objects in Cl1600+4109.
Cl 1613+3104 Cl 1600+4109 Id. Identification number --- x x coordinate number=1 coordinates with respect to the central galaxy, x increasing southward, y increasing westward arcsec y y coordinate number=1 coordinates with respect to the central galaxy, x increasing southward, y increasing westward arcsec n_B "O" if out of field for this filter --- B isophotal magnitude number=3 limiting isophote 27.0 mag/arcsec2 in Cl1613+3104 and 27.5 mag/arcsec2 in Cl1600+4109. mag n_g "O" if out of field for this filter --- g isophotal magnitude number=3 limiting isophote 27.0 mag/arcsec2 in Cl1613+3104 and 27.5 mag/arcsec2 in Cl1600+4109. mag n_r "O" if out of field for this filter --- r isophotal magnitude number=3 limiting isophote 27.0 mag/arcsec2 in Cl1613+3104 and 27.5 mag/arcsec2 in Cl1600+4109. mag n_B-g "O" if out of field for this filter --- B-g limiting isophote corresponds to g mag n_g-r "O" if out of field for this filter --- g-r limiting isophote corresponds to g mag CB Criterion B stars/galaxies number=4 Criterion to discriminate between stars and galaxies. Stars, galaxies and unclassified objects are identified respectively with 0, 2 and 1. --- Cg Criterion g stars/galaxies number=4 Criterion to discriminate between stars and galaxies. Stars, galaxies and unclassified objects are identified respectively with 0, 2 and 1. --- Cr Criterion r stars/galaxies number=4 Criterion to discriminate between stars and galaxies. Stars, galaxies and unclassified objects are identified respectively with 0, 2 and 1. --- C Final classification stars/galaxies number=5 Final classification of objects as stars (0), galaxies (2) or ambiguous (1), according to the results in columns 9 to 11. This is the criterion used in the paper by Vilchez-Gomez et al. (1995, A&A submitted). Saturated stars are identified by "5". --- Francois Ochsenbein CDS 1995 Oct 13 Roser Pello <roser@obs-mip.fr> J_A+AS_115_219.xml The Hamburg/ESO survey for bright QSOs. II. Follow-up spectroscopy of 160 quasars and Seyferts J/A+AS/115/235 J/A+AS/115/235 The Hamburg/ESO survey for bright QSOs. II. The Hamburg/ESO survey for bright QSOs. II. Follow-up spectroscopy of 160 quasars and Seyferts D Reimers T Koehler L Wisotzki Astron. Astrophys. Suppl. Ser. 115 235 1996 1996A&AS..115..235R Galaxies, Seyfert QSOs Redshifts galaxies: distances and redshifts galaxies: Seyfert quasars: general surveys We report about the first phase of a wide-angle survey for bright QSOs (12.5<~B<~17.5) in the southern hemisphere, based on objective prism plates taken with the ESO Schmidt telescope over an effective area of ~1000 sq.deg. After digitisation, the extracted spectra were searched for quasar candidates in a largely automated two-stage procedure. Several selection criteria, such as UV excess or presence of emission lines, were applied simultaneously to the databases. Thanks to the high spectral resolution of the spectra, the stellar contamination in the candidate sets could be efficiently kept low. Follow-up spectroscopy has yielded 160 newly discovered QSOs and Seyfert 1 galaxies, plus a variety of other interesting galactic and extragalactic objects. Although the present QSO sample is not statistically "complete" insofar as it has no well-defined flux limit, there is no evidence for strong redshift-dependent selection biases. The extension of the survey over an area of 5000sq.deg. and the construction of flux-limited subsamples are under way.
Coordinates, magnitudes, and redshifts of QSOs and Seyfert 1 galaxies Seq Sequence number --- HES HES name (Hamburg/ESO Survey) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec RAh1950 Right ascension (B1950) h RAm1950 Right ascension (B1950) min RAs1950 Right ascension (B1950) s DE-1950 Declination sign --- DEd1950 Declination (B1950) deg DEm1950 Declination (B1950) arcmin DEs1950 Declination (B1950) arcsec Field Field number --- bmag b magnitude mag Instr Used instrument number=1 1 = EFOSC1 at 3.6m telescope 2 = EFOSC2 at 2.2m telescope p = photographic B magnitude s = B magnitude estimated from spectrum --- z Redshift --- LabLine Laboratory line --- Telescop Telescope --- Date Date of observation (Month and Year) --- Note See Note number=2 1 Listed as ROSAT detection by Bade et al. 1995, A&AS 110, 469 =1995A&AS..110..469B 2 also Maza et al. 1992, Rev. Mex. Astron. Astrofis. 24, 147; no redshift given there =1992RMxAA..24..147M 3 also Maza et al. 1993, Rev. Mex. Astron. Astrofis. 25, 51; several of their redshifts are inaccurate or wrong =1993RMxAA..25...51M 4 also Maza et al. 1994, Rev. Mex. Astron. Astrofis. 28, 187, assuming their 1950 coordinates are in fact J2000; no redshift given there =1994RMxAA..28..187M 5 already published by Wisotzki et al. 1991, A&A 247, L17 =1991A&A...247L..17W 6 Double QSO, position refers to bright component; already published by Wisotzki et al. 1993, A&A 278, L15 =1993A&A...278L..15W --- Simona Mei CDS 1995 Sep 07 J_A+AS_115_235.xml A catalogue of high velocity molecular outflows J/A+AS/115/283 J/A+AS/115/283 A catalogue of high velocity molecular outflows A catalogue of high velocity molecular outflows Y Wu M Huang J He Astron. Astrophys. Suppl. Ser. 115 283 1996 1996A&AS..115..283W Interstellar medium catalogs ISM: jets ISM: molecules We present a comprehensive catalogue of 264 high velocity molecular outflow sources that are compiled from publications and preprints as of May 1995, including position, bottom linewidth, maximum measurement of projected profile, polarity, collimation factor, outflow mass, luminosity and list of related references.
Outflow sources Number Source number --- Name Source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLONd Galactic longitude deg GLONm Galactic longitude arcmin GLATd Galactic latitude deg GLATm Galactic latitude arcmin l_Dist Limit flag on distance from the Sun --- Dist Distance from the Sun kpc Z Altitude from the Galactic plane pc l_DeltaV Limit flag on full linewidth --- DeltaV Full linewidth at 0.1K or 0.2K above zero temperature level number=1 In some sources, emission at extremely high velocity has been detected on the level of tens of milli-Kelvins, km/s n_DeltaV When '-' there is a range of values --- DeltaV2 Second value of full linewidth km/s Polarity Polarity number=2 Bi: bipolar outflow MB: blue monopolar outflow MR: red monopolar outflow Mul: outflow is multipolar Iso: the outflow is isotropic --- l_Rmax Limit flag on major axis --- Rmax Linear measurement of major axis of the source pc l_Rcoll Limit or uncertainty flag on collimation factor --- Rcoll Collimation factor of outflow --- n_Rcoll When 'r' the value of the collimator factor is quoted from the references --- l_MOutFlow Limit or uncertainty label on outflow mass --- MOutFlow Outflow mass determined by integrating CO emission of the entire area of the wings (Lada 1985) or lower value of outflow mass when there is a range of values solMass MOutFlow2 Upper value for outflow mass when there is a range of values solMass n_MOutFlow See Note number=3 The masses calculated under "optical thick" are noted with "h". The others were drived mainly with one CO transition or not in "optical thick". --- l_Lum Limit or uncertainty flag on luminosity --- Lum The bolometric luminosity of associate stellar source which is measured mainly by infrared photometry or integrated from the IRAS data solLum n_Lum When '?' uncertainty --- n_Lum2 Interval label --- Lum2 Upper value of bolometric luminosity when an interval of values is given or second value for the luminosity solLum u_Lum2 When '?' uncertainty --- Ref The publications providing the data of the object number=4 1: Bally & Lada 1983 (1983ApJ...265..824B) 2: Canto et al.1984 (1984ApJ...282..631C) 3: Snell et al.1990 (1990ApJ...352..139S) 4: Brackmann & Scoville 1980 (1980ApJ...242..112B) 5: Arquilla & Goldsmith 1984 (1984ApJ...279..664A) 6: Nakano & Yoshida 1986 (1986PASJ...38..531N) 7: Lada 1985 8: Levreault 1985 9: Bachiller et al.1990b (1990A&A...231..174B) 10: Lada & Harvey 1981 (1981ApJ...245...58L) 11: Snell et a.1984 (1984ApJ...284..176S) 12: Levreault 1988 (1988ApJS...67..283L) 13: Mao et al.1989 14: Goldsmith et al.1984 (1984ApJ...286..599G) 15: Yamashita et al.1989 (1989ApJ...347..894Y) 16: Phillips et al.1988 (1988A&A...190..289P) 17: Edwards & Snell 1984 (1984ApJ...281..237E) 18: Edwards & Snell 1983 (1983ApJ...270..605E) 19: Snell & Edwards 1981 (1981ApJ...251..103S) 20: Beichman et al.1984 (1984ApJ...278L..45B) 21: Goldsmith et al.1986 (1986ApJ...303L..11G) 22: Myers et al.1988 (1988ApJ...324..907M) 23: Myers et al.1987 (1987ApJ...319..340M) 24: Heyer et al.1987 (1987ApJ...321..370H) 25: Snell et al.1980 (1980ApJ...239L..17S) 26: Strom et al.1976 (1976AJ.....81..320S) 27: Lichten 1982a (1982ApJ...255L.119L) 28: Beichman et al.1986 (1986ApJ...307..337B) 29: Liljestrom et al.1989 (1989A&A...210..337L) 30: Frerking & Langer 1982 (1982ApJ...256..523F) 31: Wu et al.1992 (1992ApJ...394..196W) 32: Snell et al.1988 (1988ApJ...325..853S) 33: Fukui et al.1986 (1986ApJ...311L..85F) 34: Morgan & Bally 1991 (1991ApJ...372..505M) 35: Ziurys et al. 1990 (1990ApJ...356L..25Z) 36: Verdes-Montenegro et al.1989 (1989ApJ...346..193V) 37: Schimid-Burgk et al.1989 (1989A&A...215..150S) 38: Erickson et al.1982 (1984ApJ...281..237E) 39: Kwan & Scoville 1976 (1976ApJ...210L..39K) 40: Olofsson et al.1982 (1982A&A...113L..18O) 41: Zuckerman et al.1976 (1975ApJ...199L..35Z) 42: Hilton et al.1986 (1986A&A...154..274H) 43: Snell & Edwards 1982 (1982ApJ...259..668S) 44: Campbell & Thompson 1984 (1984ApJ...279..650C) 45: Bally 1982 (1981ApJ...251..639B) 46: Lichten 1982b (1982ApJ...253..593L) 47: Margulis et al.1988 (1988ApJ...333..316M) 48: Haschick et al.1981 (1981ApJ...244...76H) 49: Rodriguez et al.1982 (1982ApJ...260..635R) 50: Blitz & Thaddeus 1980 (1980ApJ...241..676B) 51: Lada & Gautier 1982 (1982ApJ...261..161L) 52: Levreault 1983 (1983ApJ...265..855L) 53: Margulis & Lada 1986 (1986ApJ...309L..87M) 54: Dent et al. 1984 (1984MNRAS.210..173D) 55: Rodriguez et al.1980 (1980ApJ...240L.149R) 56: Tamura et al.1990 (1990ApJ...350..728T) 57: Fischer et al.1982 (1982ApJ...258..165F) 58: Simon et al.1984 (1984ApJ...278..170S) 59: Heyer et al.1986 (1986ApJ...308..134H) 60: Ho et al.1982 (1982ApJ...262..619H) 61: Armstrong & Winnewisser 1989 (1989A&A...210..373A) 62: Edwards & Snell 1982 (1982ApJ...261..151E) 63: Little et al.1988 (1988A&A...205..129L) 64: Lada et al.1984 (1984ApJ...286..302L) 65: Dickel et al. 1978 (1978ApJ...223..840D) 66: Levreault 1984 (1984ApJ...277..634L) 67: White & Phillips 1981 (1981MNRAS.194..947W) 68: Sato & Fukui 1989 (1989ApJ...343..773S) 69: Mathieu et al.1988 (1988ApJ...330..385M) 70: Rodriguez et al.1981 (1981AJ.....86.1245R) 71: Haikala & Laureijs 1989 (1989A&A...223..287H) 72: Dent et al.1985 (1985MNRAS.217..217D) 73: Little et al.1985 (1985MNRAS.217..227L) 74: Canto et al.1981 (1981ApJ...244..102C) 75: Reipurth & Olberg 1991 (1991A&A...246..535R) 76: Kameya et al.1988 (1989ApJ...339..222K) 77: Evans et al.1981a (1981ApJ...246..409E) 78: Harvey et al.1984 (1984ApJ...278..156H) 79: Schwartz et al.1983 (1983ApJ...271..625S) 80: Calvet et al.1983 (1983ApJ...268..739C) 81: Wolf et al.1990 (1990AJ....100.1892W) 82: Hayashi et al.1987 (1987ApJ...312..327H) 83: Evans et al.1981b (1981ApJ...250..200E) 84: Terebey et al.1989 (1989ApJ...340..472T) 85: Yang et al.1990 (1990ApJ...362..538Y) 86: Fukui 1989 87: Arquilla & Kwok 1987 (1987A&A...173..271A) 88: Fischer et al.1985 (1985ApJ...293..508F) 89: Sugitani et al.1989 (1989ApJ...342L..87S) 90: Casoli et al.1986 (1986A&A...169..281C) 91: Schwartz et al. 1988 (1988ApJ...327..350S) 92: Loren 1989 (1989ApJ...338..925L) 93: Parker et al.1988 (1988MNRAS.234...67P) 94: Harvey & Forveille 1988 (1988A&A...197L..19H) 95: Scoville et al.1986 (1986ApJ...303..416S) 96: Bachiller & Cernicharo 1990 (1990A&A...239..276B) 97: Xie & Goldsmith 1990 (1990ApJ...359..378X) 98: Clark 1986 (1986A&A...164L..19C) 99: Wouterloot et al.1989 (1989A&A...215..131W) 100: Vallee & Avery 1990 (1990A&A...233..553V) 101: Sanders & Willner 1985 (1985ApJ...293L..39S) 102: Richer 1990 (1990MNRAS.245p..24R) 103: Schmid-Burgk et al.1990 (1990ApJ...362L..25SS) 104: Yang et al.1991 (1991ApJ...373..137Y) 105: Mizuno et al.1990 (1990ApJ...356..184M) 106: Andre et al.1990 (1990A&A...236..180A) 107: Verdes-Montenegro et al.1990 (1990Ap&SS.171..161V) 108: Schwartz et al.1985 (1985ApJ...295...89S) 109: Davidson & Jaffe 1984 (1984ApJ...277L..13D) 110: Iwata et al.1988 (1988ApJ...325..372I) 111: Olberg et al.1992 (1992A&A...259..252O) 112: Mattila et al.1989 113: Smith & Fischer 1992 (1992ApJ...398L..99S) 114: Reipurth 1989 115: Reipurth & Graham 1991 116: Wilking et al.1990 (1990AJ....100..758W) 117: Heyer et al.1989 (1989ApJ...346..220H) 118: Evans et al.1994 (1994ApJ...424..793E) 119: Koo et al.1994 (1994ApJ...429..233K) 120: Phillips & Mampaso 1991 (1991A&AS...88..189P) 121: Bachiller et al.1991 (1991A&A...251..639B) 122: Umemoto et al. 1992 (1992ApJ...392L..83U) 123: Odenwald & Schwartz 1993 (1993ApJ...405..706O) 124: Ladd et al.1991 (1991ApJ...366..203L) 125: Barsony 1989 (1989ApJ...345..268B) 126: Bachiller et al.1990a (1990A&A...236..461B) 127: Chernin & Masson 1991 (1991ApJ...382L..93C) 128: Moriarty-Schieven & Wanner 1991 (1991ApJ...373L..23M) 129: Wilson & Mauersberger 1991 (1991A&A...244L..33W) 130: Knee 1992 (1992A&A...259..283K) 131: Wootten & Loren 1987 (1987ApJ...317..220W) 132: Margulis et al.1990 (1990ApJ...352..615M) 133: Fukui et al.1989 (1988ApJ...325L..13F) 134: Mendoza et al. 1990 (1990MNRAS.246..518M) 135: Liseau et al. 1988 (1988A&A...192..153L) 136: Walker et al. 1988 (1988ApJ...332..335W) 137: Kutner et al. 1982 (1982ApJ...259L..35K) 138: Fukui et al. 1989 (1989Natur.342..161F) 139: Weintraub et al.1993 (1993AJ....105..271W) 140: Loren et al.1990 (1990ApJ...365..269L) 141: Eiroa et al.1992 (1992PASJ...44..155E) 142: Tamura et al.1991 (1991ApJ...374L..25T) 143: Cohen & Schwartz 1987 (1987ApJ...316..311C) 144: Terebey et al.1990 (1990ApJ...362L..63T) 145: Morilarty-Schieven et al.1992 (1991ApJ...373L..23M) 146: Tamura et al.1991 (1991ApJ...374L..25T) 147: Margulis et al. 1989 (1989ApJ...345..906M) 148: Garden et al.1991 (1991ApJ...374..540G) 149: Umemoto et al.1991 (1991ApJ...377..510U) 150: Duvert et al.1990 (1990A&A...233..190D) 151: Koo 1989 (1989ApJ...337..318K) 152: Choi et al. 1993 (1993ApJ...417..624C) 153: Margulis & Snell 1989 (1989ApJ...343..779M) 154: Avery et al.1990 (1990ApJ...357..524A) 155: Olberg et al.1989 156: Reipurth et al.1992 (1993A&A...273..221R) 157: Armstrong 1989 158: Cohen 1980 (1980AJ.....85...29C) 159: Kenyon et al.1993 (1993AJ....105.1505K) 160: Torrelles et al.1993 (1993ApJ...410..202T) 161: Morgan et al.1993 (1991ApJ...376..618M) 162: Kazuhito 1993 (1993AJ....105.1487D) 163: Minchin et al.1993 (1993A&A...277..595M) 164: Kastner et al.1994 (1994ApJ...425..695K) 165: Bally et al.1994 (1994ApJ...423..310B) 166: Hasegawa et al.1994 (1994ApJ...426..215H) 167: White 1993 (1993A&A...274L..33W) 168: Parker et al.1991 (1991MNRAS.252..442P) 169: Blake et al.1995 (1995ApJ...441..689B) 170: Minchin et al.1995 (1995A&A...293L..61M) 171: Sato, et al.1994 (1994ApJ...435..279S) 172: Wu, et al.,1995 173: Zilik, et al.,1978 (1978ApJ...222..896Z) 174: Masson et al.1990 (1990ApJ...357L..25M) 175: Chernin & Masson 1992 (1992ApJ...396L..35C) 176: Haikala & Dietrich 1989 177: Bourke,1995 178: Yun & Clemens 1992 (1992ApJ...385L..21Y) 179: Wang et al. 1995 (1995ApJ...454..217W) 180: Dobashi et al. 1994 (1994AJ....107.2148D) --- table.tex LaTeX version of table1 Simona Mei, Francois Ochsenbein CDS 1996 Dec 04 UNKNOWN UNKNOWN * 06-Sep-1995: prepared by Simona Mei * 04-Dec-1996: Two corrections in the table were performed at the author's request <wuyf@bao01.bao.ac.cn> on sources 239 (reference) and 45 (mass). Bibcodes were added in Note (4). J_A+AS_115_283.xml A catalogue of massive young stellar objects J/A+AS/115/285 J/A+AS/115/285 Catalogue of massive young stellar objects A catalogue of massive young stellar objects S J Chan T Henning K Schreyer Astron. Astrophys. Suppl. Ser. 115 285 1996 1996A&AS..115..285C Photometry, infrared Radio lines YSOs catalogs infrared: stars radio continuum: ISM radio lines: ISM stars: formation A catalogue of massive young stellar objects which contains about 250 objects is presented. This catalogue is an updated version of the catalogue of Henning et al. (1984). It provides comprehensive information on infrared and radio flux densities, molecular line data, association with maser sources, and outflow phenomena.
The basic data IRAS IRAS name --- Name Name of the object --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLON Galactic longitude of the object deg GLAT Galactic latitude of the object deg Sp Spectral type --- OtherNam Other Names --- The basic data (distances and references) IRAS IRAS name --- l_Dist Limit flag on distance --- Dist Kinematic distance of the object kpc Dist2 Second value of distance if an interval of values is given kpc Refer References (See References on refs file) --- The flux densities in the near-infrared (J,H,K) and submillimeter/millimeter data IRAS IRAS name --- Detect Number of detections --- DiffDist Distance difference between the infrared source and our selected IRAS object arcmin CIO Name of the infrared source from the Catalogue of Infrared Observations (Gezari D.Y. 1994) --- x_Flux Flux measurement unit (Gezari D.Y. 1994) --- Beam Angular beam size --- x_Beam Angular beam size measurement unit number=1 s: arcsec; m: arcmin; V: varied (reader should refer to the original paper for details) --- Beam2 Second value for angular beam size --- x_Beam2 Measurement unit of the second value for angular beam size number=1 s: arcsec; m: arcmin; V: varied (reader should refer to the original paper for details) --- UpBeam2 Upper value for Beam2 when an interval of values is given --- x_UpBeam2 Measurement unit of the upper value for Beam2 number=1 s: arcsec; m: arcmin; V: varied (reader should refer to the original paper for details) --- JFlux Flux density at J (1.25 micron) in x_Flux --- HFlux Flux density at H (1.65 micron) in x_Flux --- KFlux Flux density at K (2.2 micron) in x_Flux --- Flux350 Flux density at 350 micron in x_Flux --- Flux800 Flux density at 800 micron in x_Flux --- Flux1300 Flux density at 1300 micron in x_Flux --- CIORef CIO reference number --- Referen References (See References numbers on refs file) --- Remarks Special remarks on the data --- The flux density at 6 cm IRAS IRAS name --- l_Flux Limit symbol on flux --- Flux Flux density at 6 cm in x_Flux --- u_Flux Uncertainty flag on Flux --- e_Flux Error on Flux in x_Flux --- Flux2 Second value for Flux --- x_Flux Flux and flux error unit in Jy, mJy or mJy/23" --- Referen References (See References numbers on refs file) --- Remarks Special remarks on measurements --- IRAS data IRAS IRAS name --- Flux12 Flux density in the 12 micron band Jy Flux25 Flux density in the 25 micron band Jy Flux60 Flux density in the 60 micron band Jy Flux100 Flux density in the 100 micron band Jy q_Flux12 Flux quality in the 12 micron band --- q_Flux25 Flux quality in the 25 micron band --- q_Flux60 Flux quality in the 60 micron band --- q_Flux100 Flux quality in the 100 micron band --- e_Flux12 Relative uncertainty of flux densities in the 12 micron band % e_Flux25 Relative uncertainty of flux densities in the 25 micron band % e_Flux60 Relative uncertainty of flux densities in the 60 micron band % e_Flux100 Relative uncertainty of flux densities in the 100 micron band % Var IRAS variability --- R(12/25) IRAS colours of the objects (12 micron and 25 micron) number=1 R(i/j)=log(iF(j)/jF(i)) --- R(25/60) IRAS colours of the objects (25 micron and 60 micron) number=1 R(i/j)=log(iF(j)/jF(i)) --- R(60/100) IRAS colours of the objects (60 micron and 100 micron) number=1 R(i/j)=log(iF(j)/jF(i)) --- LRS LRS class of the object --- The information on dust features (ice, silicate and PAH (polycyclic aromatic hydrocarbon (Allamandola et al. 1989)) IRAS IRAS name --- PAH3.3 Presence of the PAH (Polycyclic aromatic hydrocarbon) emission features at 3.3 micron number=1 Y : feature present N : no feature present ? : feature possibly present --- PAH7.7 Presence of the PAH emission features at 7.7 micron number=1 Y : feature present N : no feature present ? : feature possibly present --- PAH8 Presence of the PAH emission features at 8.6/8.7 micron number=1 Y : feature present N : no feature present ? : feature possibly present --- PAH11.3 Presence of the PAH emission features at 11.3 micron number=1 Y : feature present N : no feature present ? : feature possibly present --- r_PAH Reference which provide the information on PAH features (See References numbers on refs file) --- Sil10 Silicate absorption feature at 9.7/10 micron --- Sil18 Silicate absorption feature at 18 micron --- r_Sil Reference which provide the information on silicate absorption features (See References numbers on refs file) --- Ice3.08 Ice absorption feature at 3.08 micron --- r_Ice Reference number of literature which provide the information on ice absorption features (See References numbers on refs file) --- Water Maser data IRAS IRAS name --- Det Detection number=1 D: Detection N: Non detection O: Observed without any detection --- n_Det Uncertainty on detection --- Telescop Telescope used during the observing runs (the information on this telescope is in Table 12) --- Beam Angular beam size of the observation or, in case of a rectangular beam, first dimension of the beam --- Beam2 In case of a rectangular beam, second dimension of the beam --- x_Beam Beam Units (S=arcsec, M=arcmin) --- r_Beam References (See References numbers on refs file) --- Type Character of the line: M=maser --- Comment Special remarks on the measurement --- OH data CH3OH maser/line data NH3 line data CS line data HCO+ or HCO line data IRAS IRAS name --- Det Detection number=1 D: Detection N: Non detection --- n_Det Uncertainty on detection --- Telescop Telescope used during the observing runs (the information on this telescope is in Table 12) --- Beam Angular beam size of the observation or, in case of a rectangular beam, first dimension of the beam --- Beam2 In case of a rectangular beam, second dimension of the beam --- x_Beam Beam Units (S=arcsec, M=arcmin, A=mas (milliarcsec)) --- r_Beam References (See References numbers on refs file) --- Trans Transition of the line --- Freq Line in this transition at a particular frequency MHz Sep Separation flag --- Freq2 Second value of line in this transition at a particular frequency MHz Line Character of the line number=2 M=maser E=emission A=absorption --- n_Line Uncertainty on character of the line --- Line2 Character of the second value of line --- Remarks Special remarks on the measurements --- CO line data IRAS IRAS name --- Det Detection (D) or non-detection (N) --- Telescop Telescope used during the observing runs (the information on this telescope is in Table 12) --- Beam Angular beam size of the observation or, in case of a rectangular beam, first dimension of the beam --- Beam2 In case of a rectangular beam, second dimension of the beam --- x_Beam Beam Units (S=arcsec, M=arcmin) --- r_Beam References (See References numbers on refs file) --- Trans Transition of the line --- Freq The frequency of the line MHz DeltaV FWHM of the line km/s e_DeltaV Uncertainty on the FWHM of the line km/s MinV Minimum velocity at which an emission has been observed km/s MaxV Maximum velocity at which an emission has been observed km/s Remarks Special remarks on the measurements --- The information of telescopes during the observations Telescop Abbreviated name of the observatory --- Observ Observatory name --- City City where the observatory is located --- Country Country where the observatory is located --- Summary of the observational information on molecules - maser Summary of the observational information on molecules of the 'confused objects' - maser IRAS IRAS name --- H2O Water maser at 22.235 GHz --- n_H2O Uncertainty on detection --- OH1612 OH maser at 1612 MHz --- OH1665 OH maser at 1665 MHz --- OH1667 OH maser at 1667 MHz --- OH1720 OH maser at 1720 MHz --- OH4660 OH maser at 4660 MHz --- OH4750 OH maser at 4750 MHz --- OH4765 OH maser at 4765 MHz --- OH6030 OH maser at 6030 MHz --- OH6035 OH maser at 6035 MHz --- CH3OH6 CH3OH maser/line at 6.668 GHz --- CH3OH12 CH3OH maser/line at 12.179 GHz --- CH3OH28 CH3OH maser/line at 28.3 GHz --- CH3OH36 CH3OH maser/line at 36.169 GHz --- CH3OH37 CH3OH maser/line at 37.703 GHz --- CH3OH44 CH3OH maser/line at 44.069 GHz --- CH3OH48 CH3OH maser/line at 48.372 GHz --- CH3OH88 CH3OH maser/line at 88.6 GHz --- Summary of the observational information molecules - molecular lines Summary of the observational information on molecules of the 'confused objects' - molecular lines IRAS IRAS name number= D: Detection N: Non-detection O: Observed without any detection --- CS48 CS line at 48.99 GHz number= D: Detection N: Non-detection O: Observed without any detection --- CS97 CS line at 97.98 GHz number= D: Detection N: Non-detection O: Observed without any detection --- CS244 CS line at 244.94 GHz number= D: Detection N: Non-detection O: Observed without any detection --- CS342 CS line at 342.88 GHz number= D: Detection N: Non-detection O: Observed without any detection --- C34S C^34^S line at 96.41 GHz number= D: Detection N: Non-detection O: Observed without any detection --- NH3-23.6 NH3 line at 23.69 GHz number= D: Detection N: Non-detection O: Observed without any detection --- n_NH3-23.6 Uncertainty on detection number= D: Detection N: Non-detection O: Observed without any detection --- NH3-23.7 NH3 line at 23.72 GHz number= D: Detection N: Non-detection O: Observed without any detection --- n_NH3-23.7 Uncertainty on detection number= D: Detection N: Non-detection O: Observed without any detection --- NH3-24.1 NH3 line at 24.139 GHz number= D: Detection N: Non-detection O: Observed without any detection --- NH3-24.5 NH3 line at 24.532 GHz number= D: Detection N: Non-detection O: Observed without any detection --- HCO+ 89 [DN] HCO+ line at 89.19 GHz number= D: Detection N: Non-detection O: Observed without any detection --- CO115 CO line at 115.27 GHz number= D: Detection N: Non-detection O: Observed without any detection --- CO230 CO line at 230.54 GHz number= D: Detection N: Non-detection O: Observed without any detection --- CO345 CO line at 345.8 GHz number= D: Detection N: Non-detection O: Observed without any detection --- 13CO110 ^13^CO line at 110.2 GHz number= D: Detection N: Non-detection O: Observed without any detection --- 13CO220 ^13^CO line at 220.4 GHz number= D: Detection N: Non-detection O: Observed without any detection --- refs.tex References in LaTeX Simona Mei CDS 1995 Jul 28 J_A+AS_115_285.xml Astrometry of outer Jovian satellites from The Uppsala-ESO Survey of Asteroids and Comets (UESAC) J/A+AS/115/295 J/A+AS/115/295 Astrometry of outer Jovian satellites Astrometry of outer Jovian satellites from The Uppsala-ESO Survey of Asteroids and Comets (UESAC) O Hernius C -I Lagerkvist M Lindgren G V Williams G Tancredi Astron. Astrophys. Suppl. Ser. 115 295 1996 1996A&AS..115..295H Solar system astrometry planets and satellites: individual (satellites of Jupiter) In the course of The Uppsala-ESO Survey of Asteroids and Comets astrometric positions of the faint outer Jovian satellites J VI-XIII were obtained from photographic plates and films taken at the European Southern Observatory, La Silla, Chile and at the Anglo-Australian Observatory, Siding Spring, Australia
Observed astrometric positions of the Jovian satellites Satellite Satellite identification --- Year Year of observation yr Month Month of observation "month" Day Day of observation d RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec e_RAs Error on right ascension arcsec e_DEs Error on declination arcsec Expos Exposure length min PlatEm Plates emulsion --- Observ Observatory code --- Simona Mei CDS 1995 Sep 07 J_A+AS_115_295.xml The central field of Omega Centauri J/A+AS/115/297 J/A+AS/115/297 BVRI photometry of Central Field of Omega Cen The central field of Omega Centauri G Lynga Astron. Astrophys. Suppl. Ser. 115 297 1996 1996A&AS..115..297L Clusters, globular Photometry, BVRI blue stragglers globular clusters: individual (Omega Cen) Hertzsprung-Russell (HR diagram) stars: horizontal-branch This is a four colour photometric study of stars in the central part of the globular cluster Omega Centauri. A CCD has been used and the observations were made at Siding Spring Observatory.
Bright stars in the centre of omega Centauri; V<12.00 Blue stars in the centre of omega Centauri; B-V <= 0.1; if B not measured: V-R <=0.2 and V-I confirming blue colour BVRI photometry and equatorial positions for stars in the centre of Omega Centauri Id Identification number number=1 No. 1466 and 2073 coincide with UIT-1 and UIT-2 (Landsman et al., 1992) --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Vmag V magnitude mag e_Vmag Error on V magnitude mag B-V B-V colour index mag e_B-V Error on B-V mag V-R V-R colour index mag e_V-R Error on V-R mag V-I V-I colour index mag e_V-I Error on V-I mag Dist Distance from the centre of the cluster as defined in the paper arcsec Simona Mei CDS 1995 Aug 01 J_A+AS_115_297.xml Four-colour photometry of eclipsing binaries. XXXVII. Light curves of the B-type system V539 Arae J/A+AS/115/315 J/A+AS/115/315 uvby light curves of the system V539 Arae Four-colour photometry of eclipsing binaries. XXXVII. Light curves of the B-type system V539 Arae J V Clausen J M Garcia A Gimenez B E Helt K S Jensen J Suso L P R Vaz Astron. Astrophys. Suppl. Ser. 115 315 1996 1996A&AS..115..315C Binaries, eclipsing Photometry, uvby binaries: eclipsing binaries: spectroscopic stars: individual (V359 Ara, HR 6614, HR 6632) stars: oscillations Accurate uvby light curves of the southern, detached, double-lined eclipsing binary V539 Ara (HR 6622A, HD 161783, V=5.71mag , B3V+B4V, P=3.17d) are presented. They contain 1409 observations in each colour, collected 1982-1984. Typical mean errors are 0.003-0.004mag. Observations for 8 additional times of minima from 1985-1994 are included. The secondary component belongs to the group of slowly pulsating B (or SPB) stars. An analysis of V539 Ara based on the new photometry and the spectroscopic orbit by Andersen (1983A&A...118..255A) is published separately (Clausen 1995).
V539 Ara HR 6622 HD 161783 IDS 17423-5335 A 17 50 28.2 -53 36 46 HR 6614 HD 161420 17 48 38.0 -55 24 08
Light curves V539 Ara - HR6614 in the 1982-1984 instrumental system (uvby) Magnitude differences V539 Ara - HR6614 in the 1985-1994 instrumental system (uvby) for 8 additional times of minima HJD Julian date d ymag y magnitude mag b-y b-y colour index mag m1 m1 index mag c1 c1 index mag bmag b magnitude mag vmag v magnitude mag umag u magnitude mag Simona Mei CDS 1995 Sep 06 J_A+AS_115_315.xml A new study of the young open cluster NGC 7510 J/A+AS/115/325 J/A+AS/115/325 UBV photometry in the cluster NGC 7510 A new study of the young open cluster NGC 7510 R Barbon S M Hassan Astron. Astrophys. Suppl. Ser. 115 325 1996 1996A&AS..115..325B Clusters, open Photometry, UBV Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 7510) stars: distances Three-colour photographic photometry of the young open cluster NGC 7510 based upon UBV observations made with the 122cm and 182cm Asiago reflectors is presented here. A mean colour excess E(B-V)=1.12, a distance of 3.09kpc could be achieved for this cluster and 31 stars could be identified as photometric physical members. An age of 10^7^years has been derived by comparison with standard isochrones. The discrepancy between the photometric and spectroscopic distances obtained for some stars is discussed and comparisons with recent investigations of the same object are also given.
NGC 7510 C 2309+603 23 11.5 +60 34
Photometry of NGC 7510 Star Star identification number as in Fig. 1 of the paper --- Vmag V magnitude mag B-V B-V color index mag u_B-V Uncertainty flag on B-V color index --- U-B U-B color index mag u_U-B Uncertainty flag on B-V color index --- Member The letter "m" denotes a probable physical member of the cluster --- Simona Mei CDS 1995 Sep 18 J_A+AS_115_325.xml Grid of stellar models. VI. Horizontal branch and early asymptotic giant branch for low mass stars (Z=0.020, 0.001). J/A+AS/115/339 J/A+AS/115/339 Stellar models VI. Grid of stellar models. VI. Horizontal branch and early asymptotic giant branch for low mass stars (Z=0.020, 0.001). C Charbonnel G Meynet A Maeder D Schaerer Astron. Astrophys. Suppl. Ser. 115 339 1996 1996A&AS..115..339C J/A+AS/96/269 : (I) z=0.01, 0.02 (Schaller et al., 1992) J/A+AS/98/523 : (II) z=0.008 (Schaerer et al., 1992) J/A+AS/101/415 : (III) z=0.004 (Charbonnel et al., 1993) J/A+AS/102/339 : (IV) z=0.04 (Schaerer et al., 1993) J/A+AS/103/97 : (V) z=0.001, 0.004, 0.008, 0.020 and 0.040 (Meynet et al., 1994) Models, evolutionary Hertzsprung-Russell (HR diagram) stars: AGB and post-AGB stars: evolution stars: horizontal-branch New grids of models covering the evolution of low mass stars (0.8 to 1.7M_{sun}_) with metallicities Z=0.020 and 0.001 from the zero age main sequence up to the end of the early asymptotic giant branch are presented. The evolutionary tracks have been calculated with the new OPAL radiative opacities by Iglesias & Rogers (1993) and Kurucz (1991). They complete the base of extensive grids of stellar models computed by the Geneva Group with up-to-date input physics (Schaller et al. 1992; Schaerer et al. 1992; Charbonnel et al. 1993; Schaerer et al. 1993; Meynet et al. 1994).
0.8 M, Z=0.001, no overshooting, std mass loss 1.5 M, Z=0.001, with overshooting (0.20) 1.5 M, Z=0.001, no overshooting, std mass loss 1.5 M, Z=0.020, with overshooting (0.20) 1.5 M, Z=0.020, no overshooting, std mass loss 1.7 M, Z=0.001, with overshooting (0.20) 1.7 M, Z=0.001, no overshooting, std mass loss 1.7 M, Z=0.020, with overshooting (0.20) 1.7 M, Z=0.020, no overshooting, std mass loss 0.8 M, Z=0.020, no overshooting, std mass loss 0.9 M, Z=0.001, no overshooting, std mass loss 0.9 M, Z=0.020, no overshooting, std mass loss 1.0 M, Z=0.020, no overshooting, std mass loss 1.25M, Z=0.020, no overshooting, std mass loss 1.25M, Z=0.001, no overshooting, std mass loss No Number of selected point --- Age Age yr Mass Actual mass solMass log(L) Luminosity solLum log(T) Effective temperature K Hs H surface abundance (mass fraction) --- Hes He surface abundance (mass fraction) --- 12Cs 12C surface abundance (mass fraction) --- 13Cs 13C surface abundance (mass fraction) --- 14Ns 14N surface abundance (mass fraction) --- 16Os 16O surface abundance (mass fraction) --- 17Os 17O surface abundance (mass fraction) --- 18Os 18O surface abundance (mass fraction) --- 20Nes 20Ne surface abundance (mass fraction) --- 22Nes 22Ne surface abundance (mass fraction) --- Mcore Core mass fraction --- log(Teff) Uncorrected Teff (WR stars only) K log(dM/dt) Mass loss rate solMass/yr log(rho) Central density g/cm3 log(Tc) Central temperature K Hc H central abundance (mass fraction) --- Hec He central abundance (mass fraction) --- 12Cc 12C central abundance (mass fraction) --- 13Cc 13C central abundance (mass fraction) --- 14Nc 14N central abundance (mass fraction) --- 16Oc 16O central abundance (mass fraction) --- 17Oc 17O central abundance (mass fraction) --- 18Oc 18O central abundance (mass fraction) --- 20Nec 20Ne central abundance (mass fraction) --- 22Nec 22Ne central abundance (mass fraction) --- Patricia Bauer CDS 1996 Jan 12 C. Charbonnel <corinne@srvdec.obs-mip.fr> J_A+AS_115_339.xml Radio sources in fields centered near supernova remnant G160.9+2.6 (HB9) J/A+AS/115/345 J/A+AS/115/345 Radio sources in fields near G160.9+2.6 Radio sources in fields centered near supernova remnant G160.9+2.6 (HB9) D A Leahy R S Roger Astron. Astrophys. Suppl. Ser. 115 345 1996 1996A&AS..115..345L Radio sources catalogs radio continuum: general surveys We present a catalogue of the 408MHz and 1420MHz radio sources in the region centered near Right Ascension 4h58m and Declination 46degrees (epoch 1950), i.e. near the supernova remnant HB9. The observations were made with the Synthesis Telescope at the Dominion Radio Astrophysical Observatory, near Penticton, Canada. 494 sources at 408MHz and 255 sources at 1420MHz were detected. 408-1420MHz spectral indices for 101 common sources were derived. The 408MHz source list was compared with the 4850MHz sources from the Green Bank catalog. Spectral indices were determined for 165 common sources. We also compared the source lists with the IRAS and ROSAT point source catalogs for that region and have identified 16 radio sources with IRAS point sources and 3 radio sources with X-ray sources.
408 MHz Source List 1420 MHz Source List n_Source See Note number=1 When '*': Below 10% level of primary polar diagram --- Source Source Designation --- RAh Right Ascension (1950) h RAm Right Ascension (1950) min RAs Right Ascension (1950) s e_RAs Right Ascension Error s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec e_DEs Declination Error arcsec Flux Flux density mJy e_Flux Flux error mJy Majaxis Major axis arcmin Minaxis Minor axis arcmin PA Position angle deg Ident Associated source(s) number=2 21 cm source(s) in Table 2; 74 cm source in Table 3. Sources listed in brackets indicate positional discrepancies exceeding 1.5'. --- 408 MHz - 1420 MHz spectral indices 408 MHz - 4850 MHz spectral indices Source Source name --- n_Source See Note number=1 When '*' source is possibly extended at 1420 MHz; integrated flux density was used for spectral index --- Alpha Spectral index --- e_Alpha Error on spectral index --- IRAS sources with counterparts at 408 or 1420 MHz IRAS IRAS number --- Flux12 Flux at 12 {mu}m Jy Flux25 Flux at 25 {mu}m Jy Flux60 Flux at 60 {mu}m Jy Flux100 Flux at 100 {mu}m Jy Source 408 or 1420MHz Source number --- Simona Mei CDS 1995 Sep 18 J_A+AS_115_345.xml Stark broadening spectral lines of multicharged ions of astrophysical interest. XIII. C V and P V J/A+AS/115/351 J/A+AS/115/351 Stark broadening. XIII. C V and P V Stark broadening spectral lines of multicharged ions of astrophysical interest. XIII. C V and P V M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 115 351 1996 1996A&AS..115..351D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar MgI lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles molecular data Using a semiclassical approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 25 C V and 51 P V multiplets.
Stark broadening parameters due to e-, p- and He III-impacts for C V and P V N Perturber density cm-3 El Element --- Tr Transition --- Lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We See note number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de See note number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- de Shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp See note number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp See note number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dp Shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ See note number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ See note number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dHe++ Shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Simona Mei CDS 1995 Oct 13 J_A+AS_115_351.xml uvbyHbeta photometry of main sequence A type stars J/A+AS/115/401 J/A+AS/115/401 uvby-beta photometry of A-type stars uvbyHbeta photometry of main sequence A type stars C Jordi F Figueras J Torra R Asiain Astron. Astrophys. Suppl. Ser. 115 401 1996 1996A&AS..115..401J Photometry, uvby, beta Stars, early-type Galaxy: kinematics and dynamics stars: distances stars: early-type stars: fundamental parameters We present Stroemgren uvby and H_{beta}_ photometry for a set of 575 northern main sequence A type stars, most of them belonging to the Hipparcos Input Catalogue, with V from 5mag to 10mag and with known radial velocities. These observations enlarge the catalogue we began to compile some years ago to more than 1500 stars. Our catalogue includes kinematic and astrophysical data for each star. Our future goal is to perform an accurate analysis of the kinematical behaviour of these stars in the solar neighbourhood.
Photometry of the standard stars (tables 1-4) Observ Observatory / Instrument used number=1 this number is also the table number of the publication; it has the following values: 1 = O.A.N.: 1.52m telescope of the Observatorio Astronomical Nacional, Calar Alto, Almeria, Spain 2 = C.A.H.A.: 1.23m telescope at the Centro Astronomico Hispano-Aleman Calar Alto, Almeria, Spain 3 = R.G.O., Romeo channel: Jakobus Kapteyn telescope at Observatorio del Roque de los Muchachos, Canary Islands 4 = R.G.O., Julieta channel. --- HD HD identification --- b-y b-y colour index mag e_b-y Error on b-y index mag Vmag V magnitude mag e_Vmag Error on V magnitude mag m1 m1 index mag e_m1 Error on m1 index mag c1 c1 index mag e_c1 Error on c1 index mag o_c1 Number of observations --- beta Hbeta index mag e_beta Error on Hbeta index mag o_beta Number of observations for Hbeta --- D(b-y) Difference with standard values number=2 Difference is (standard - observed) mag D(Vmag) Difference with standard values number=2 Difference is (standard - observed) mag D(m1) Difference with standard values number=2 Difference is (standard - observed) mag D(c1) Difference with standard values number=2 Difference is (standard - observed) mag D(beta) Difference with standard values number=2 Difference is (standard - observed) mag Photometric data for 575 programme stars HD/BD Identification (HD/BD) number=1 see individual notes below --- HIC Identification in Hipparcos Input Cat. <I/196> number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A --- SpType Spectral Type number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A --- b-y b-y colour index number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag e_b-y Error on b-y index number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag Vmag V magnitude number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag e_Vmag Error on V magnitude number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag m1 m1 index number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag e_m1 Error on m1 index number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag c1 c1 index number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag e_c1 Error on c1 index number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag n_c1 See Note number=2 '*' means that we performed only Hbeta for this particular star. uvby were taken from Hauck&Mermilliod catalogue --- o_c1 Number of observations number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A --- beta Hbeta index number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag e_beta Error on Hbeta index number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A mag o_beta Number of observations for Hbeta number= In the following notes, . theta = position of secondary star (units are degrees) . rho = separation between components (units are arcsec) . Delta m = difference of magnitudes between components (units are mag) HD 962 Intrinsic colours do not fit the spectral type, Hipparcos Input Catalogue quotes (B-V)=0.702 +/- 0.028 HD 3743 CCDM 00403+2403 theta=207, rho=16.3, Delta m=1.8 HD 4902 theta=30, rho=17, Delta m=4 HD 5944 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 6114 Joint photometry, CCDM 01030+4723 rho <10, Delta m=1.3, known orbit HD 10495 CCDM 01438+5553 theta=99, rho=12.8, Delta m=3.2 HD 13372 NSV 740, the V magnitudes are 6.260, 6.240, 6.223, 2SP in Renson (1991) HD 13379 Joint photometry, theta=25, rho=6, Delta m>2.5 , CL Stock 2 28 HD 13687 CL Stock 2 96 HD 13966 CL Stock 2 142 HD 17008 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 17581 SB HD 18040 theta=340, rho=20, Delta m>3 HD 23156 Joint photometry, theta=100, rho=10, Delta m>3, CL Melotte 22 158 HD 28150 CCDM 04271+1812 theta=58, rho=18.4, Delta m=1.8 HD 31326 theta=0, rho=12, Delta m=4 HD 34035 theta=300, rho=15 HD 34292 theta=330, rho=12, Delta m=4 HD 34492 Triple system, AB: theta=270, AC: theta=280, photometry of the main component HD 39181 Intrinsic colours do not fit the spectral type HD 42895 theta=235, rho=12, Delta m>4 HD 43607 theta=220, rho=12, Delta m=4 HD 46107 NGC 2244 VS 12 HD 46825 Joint photometry, CCDM 06361+1341 theta=134, rho=1.4, Delta m=5 HD 48078 theta=270, rho=12, Delta m=4 HD 48157 Joint photometry, CCDM 06421+0315 theta=150, rho=0.3, Delta m=0 HD 58383 CCDM 07260+1406 theta=195, rho=10.4, Delta m=2.0 HD 59076 Intrinsic colours do not fit the spectral type HD 67720 theta= 90, rho=12, Delta m=3.5 HD 68173 theta= 90, rho=12 HD 88987 Joint photometry, CCDM 10163+1744 rho<10, Delta m=0.2, known orbit HD 90361 Joint photometry, CCDM 10260+0256 theta=313, rho=0.4, Delta m=0.0 HD 95768 Intrinsic colours do not fit the spectral type (Jaschek (1978) quotes Am,comp) HD 99945 NSV 5230 HD 101445 Joint photometry, CCDM 11404+0057 theta=140, rho=0.9, Delta m=4.7 HD 107193 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 110500 V.R.V.? HD 123048 Joint photometry, CCDM 14046+3425 theta= 20, rho=1.9, Delta m=6.6 HD 125798 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 132029 Joint photometry, CCDM 14560+3218 theta=114, rho=4.7, Delta m=3.5 HD 133800 CCDM 15068-1629 theta=274, rho=11.1, Delta m=6.6 HD 138629 Joint photometry, CCDM 15318+4054 theta=0, rho=0.1, Delta m=0.0 HD 141458 NSV 7270, the V magnitudes are 6.785, 6.809 HD 150935 CCDM 16443-0033 theta=157, rho=13.9, Delta m=2.5 HD 154081 theta=330, rho=12, Delta m=2.5 HD 159834 CCDM 17360+2100 theta=21, rho=10.3, Delta m=3.5 HD 180638 Joint photometry, CCDM 19162+2817 theta=226, rho=1.2, Delta m=1.3 HD 180778 Quoted as Am (A2-F0) star in Renson (1991) HD 184767 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185334 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 185756 CCDM 19396+2945 theta=103, rho=11.1, Delta m=2.5 HD 186340 CCDM 19402+6030 theta=29, rho=17.5, Delta m=3.3 HD 188385 CCDM 19547+0708 theta=305, rho= 13.7, Delta m=6.0 HD 189474 Joint photometry, rho<8.0 HD 190397 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 192284 theta= 40, rho=6, Delta m=2.5, ADS 13532 A HD 192969 theta=150, rho=17, Delta m=3.5 HD 193064 Triple system, AB: theta=340, rho=26, Delta m=2, AC: theta=160, rho=12, Delta m=3 HD 193707 theta=120, rho=12, Delta m>4.0 HD 193926 CCDM 20212+4335 theta=109, rho=16.8, Delta m=2.2 HD 193984 NGC 6913 KJ 20 HD 194447 NGC 6913 KJ 147 HD 194885 Triple system, AB: theta=45, rho=17, Delta m=3, AC: theta=45, rho=36, Delta m=4 HD 195020 theta=290, rho=17, Delta m=6 HD 195479 CCDM 20310+2036 theta=63, rho=16.7, Delta m=4.0 HD 196407 Triple system, AB: theta=270, rho= 8, Delta m>4, AC: theta= 45, rho=17, Delta m>4 HD 201076 CCDM 21057+4748 theta=306, rho=11.3, Delta m=4.5 HD 201320 CCDM 21072+4744 theta=351, rho=11.4, Delta m=4.5 HD 204402 theta=135, rho=12 HD 207663 theta=265, rho=6 HD 210353 theta=190, rho=12, Delta m>4 HD 213721 Intrinsic colours do not fit the calibration for normal main sequence A type stars HD 219127 CCDM 23131+4000 theta=286, rho=14.2, Delta m=1.7 HD 220841 CCDM 23262+7041 theta=313, rho=19.9, Delta m=5.4 HD 224624 CCDM 23595+5740 theta= 76, rho=18.7, Delta m=4.0 HD 228713 theta=230, rho<10, Delta m>2, ADS 13628 AB HD 229161 NGC 6913 KJ 73 HD 236265 Joint photometry, theta=290, rho= 8, Delta m>3 HD 333092 theta=260, rho=10 BD+44 1021 theta=30, rho=6, ADS 3443 A --- Notes Notes number=3 the following symbols are used: D: information about duplicity for optical pairs with separation less than 20 arcsec. V: information about variability. B: spectroscopic binary or variable radial velocity in Renson 1991 (Catalogue general des etoiles Ap et Am, Univ de Liege, CDS Catalogue <III/162>). C: the star is member of a cluster. Identification is given in the notes. O: other remarks (see below). --- Simona Mei CDS 1995 Sep 12 J_A+AS_115_401.xml Short WSRT HI observations of spiral galaxies J/A+AS/115/407 J/A+AS/115/407 Short WSRT HI observations of spiral galaxies Short WSRT HI observations of spiral galaxies M -H Rhee T S Van Albada Astron. Astrophys. Suppl. Ser. 115 407 1996 1996A&AS..115..407R Galaxies, radio galaxies: fundamental parameters galaxies: ISM galaxies: kinematics and dynamics galaxies: spiral galaxies: structure radio lines: galaxies We have obtained short HI observations of 60 late type spiral galaxies with the Westerbork Synthesis Radio Telescope (WSRT). Several HI properties are presented, including the radial surface density distribution of HI and a position-velocity map. When possible these are compared to those measured from single-dish observations. We confirm earlier results that there is no serious systematic difference between the WSRT and single-dish observations in total flux and linewidths.
General properties of the sample galaxies Name Galaxy name --- RAh Right ascension of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database h RAm Right ascension of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database min RAs Right ascension of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database s DEd Declination of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database deg DEm Declination of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database arcmin DEs Declination of the optical center (1950) number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database arcsec MType Morphological type number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database --- Dist Distance to the galaxy number=2 Calculated from the systemic velocity (column 2 of Table 5), corrected for the Virgo-centric flow and H0=75km/s/Mpc Mpc Inclin Inclination number=3 Calculated from the axial ratio b/a of the disc: cos^2(i)=[(b/a)^2-q_0_^2]/(1-q_0_^2) deg AbB Galactic extinction in the B-band mag AiB Internal extinction in the B-band mag D25 Uncorrected blue major-axis isophotal diameter at the 25 mag/arcsec^2 number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database arcmin Dbi25 Corrected blue major-axis isophotal diameter kpc BTmag Uncorrected total apparent blue magnitude number=1 Parameters taken from LEDA, Lyon-Meudon Extragalactic Database mag MBabs Corrected absolute blue magnitude number=4 MBasb= BTmag - AbB - AiB -5log(Dist) -25 mag Observational parameters Name Galaxy name --- RAh Right ascension of the optical center (1950) h RAm Right ascension of the optical center (1950) min RAs Right ascension of the optical center (1950) s DEd Declination of the optical center (1950) deg DEm Declination of the optical center (1950) arcmin DEs Declination of the optical center (1950) arcsec ObsDay Day of observation d ObsMon Month of observation "month" ObsYear Year of observation yr ObsTime Observation length h BasMin Minimum baseline m BasMax Maximum baseline m Phi Position angle of the resolution axis deg Vobs Radial velocity of the central channel km/s BW Bandwidth of the observation MHz DeltaV Velocity spacing of the channels number=1 The velocity resolution is twice this value km/s Parameters of the position-velocity maps Name Galaxy name --- l Integration length perpendicular to the resolution axis arcmin Phi Position angle of the resolution axis deg Theta Half power beam width of the integrated antenna pattern arcsec Noise Noise level in the position-velocity map (mJy/beam) mJy HI fluxes, masses, diameters and effective surface densities Name Galaxy name --- FHI Total H I flux integral Jy.km/s MHI Total H I mass 10+9solMass DHI H I isophotal diameter at the level of 1 solMass/pc^2 kpc Reff H I effective radius, enclosing 50% of the H I mass kpc mueff H I surface density at the H I effective radius solMass/pc2 Systemic velocities and HI line profile widths Name Galaxy name --- Vsyst1 Systemic velocity determined from global profiles with the method 1 number=1 The HI profile linewidths are defined as the radial velocity differences between the high and low velocity edges, measured at the signal levels equal to 20 and 50% of: Method 1: the peak flux of the profile (e.g. Tully 1988; Bottinelli et al. 1990) Method 2: the peak fluxes in each half of the profile, separately; Method 3: the average of the peak fluxes in the two halves of the profile (e.g. Sullivan et al. 1981; Bothun et al. 1985) Method 4: the mean flux of the profile (e.g. Haynes and Giovanelli 1984; Bicay and Giovanelli 1986) km/s e_Vsyst1 Error on Systemic velocity km/s LW201 H I linewidth determined from method 1 (1), W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW201 Error on W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW501 H I linewidth determined from method 1 (1), W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW501 Error on W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s Vsyst2 Systemic velocity determined from global profiles with the method 2 number=1 The HI profile linewidths are defined as the radial velocity differences between the high and low velocity edges, measured at the signal levels equal to 20 and 50% of: Method 1: the peak flux of the profile (e.g. Tully 1988; Bottinelli et al. 1990) Method 2: the peak fluxes in each half of the profile, separately; Method 3: the average of the peak fluxes in the two halves of the profile (e.g. Sullivan et al. 1981; Bothun et al. 1985) Method 4: the mean flux of the profile (e.g. Haynes and Giovanelli 1984; Bicay and Giovanelli 1986) km/s e_Vsyst2 Error on Systemic velocity km/s LW202 H I linewidth determined from method 2 (1), W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW202 Error on W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW502 H I linewidth determined from method 2 (1), W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW502 Error on W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s Vsyst3 Systemic velocity determined from global profiles with the method 3 number=1 The HI profile linewidths are defined as the radial velocity differences between the high and low velocity edges, measured at the signal levels equal to 20 and 50% of: Method 1: the peak flux of the profile (e.g. Tully 1988; Bottinelli et al. 1990) Method 2: the peak fluxes in each half of the profile, separately; Method 3: the average of the peak fluxes in the two halves of the profile (e.g. Sullivan et al. 1981; Bothun et al. 1985) Method 4: the mean flux of the profile (e.g. Haynes and Giovanelli 1984; Bicay and Giovanelli 1986) km/s e_Vsyst3 Error on Systemic velocity km/s LW203 H I linewidth determined from method 3 (1), W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW203 Error on W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW503 H I linewidth determined from method 3 (1), W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW503 Error on W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s Vsyst4 Systemic velocity determined from global profiles with the method 4 number=1 The HI profile linewidths are defined as the radial velocity differences between the high and low velocity edges, measured at the signal levels equal to 20 and 50% of: Method 1: the peak flux of the profile (e.g. Tully 1988; Bottinelli et al. 1990) Method 2: the peak fluxes in each half of the profile, separately; Method 3: the average of the peak fluxes in the two halves of the profile (e.g. Sullivan et al. 1981; Bothun et al. 1985) Method 4: the mean flux of the profile (e.g. Haynes and Giovanelli 1984; Bicay and Giovanelli 1986) km/s e_Vsyst4 Error on Systemic velocity km/s LW204 H I linewidth determined from method 4 (1), W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW204 Error on W20 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW504 H I linewidth determined from method 4 (1), W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s e_LW504 Error on W50 number=2 W20 = the 20% level linewidth W50 = the 50% level linewidth km/s LW201c H I linewidth determined from method 1 (1), W20 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW501c H I linewidth determined from method 1 (1), W50 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW202c H I linewidth determined from method 2 (1), W20 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW502c H I linewidth determined from method 2 (1), W50 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW203c H I linewidth determined from method 3 (1), W20 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s LW503c H I linewidth determined from method 3 (1), W50 corrected for instrumental broadening number=3 W_l_ = W_l,obs_ - F_l_(r) = W_l,obs_ + (a x l + b) x r km/s Maximum rotation velocities Name Galaxy name --- Vmax.sini Maximum rotation velocity, uncorrected for inclination km/s e_Vmax.sini Error on maximum rotation velocity, uncorrected for inclination km/s Vmax Maximum rotation velocity, corrected for inclination km/s Simona Mei CDS 1995 Sep 25 J_A+AS_115_407.xml Photometric and spectroscopic studies of cool stars discovered in EXOSAT X-ray images. III. Photometric properties J/A+AS/115/41 J/A+AS/115/41 UBV Photometric and spectroscopic studies of cool stars discovered in EXOSAT X-ray images. III. Photometric properties G Cutispoto G Tagliaferri R Pallavicini L Pasquini M Rodono Astron. Astrophys. Suppl. Ser. 115 41 1996 1996A&AS..115...41C Photometry, UBVRI Stars, late-type X-ray sources stars: activity stars: late-type stars: variables: general X-rays: stars We present high-precision UBV(RI)_c_ photometry for a sample of active stars detected serendipitously by the EXOSAT satellite. Fourteen objects, out of 47 likely optical counterparts, turned out to be clearly variable, with periods in the range 1-8 days, including a newly discovered eclipsing binary. For most of them the optical variability is consistent with the presence of photospheric cool spots. We have used our multicolour photometry to estimate spectral classifications and distances. The derived distances indicate that some of the observed stars are previously unidentified nearby (d<=25pc) M dwarfs. When combined with the results of high resolution spectroscopy, our photometric observations allow us to investigate the stellar content of the selected X-ray sample. Young stars and RS CVn-type binaries appear to constitute a large fraction of the selected sample. For a description of the UBV and (RI)c photometric systems, see e.g. <http://obswww.unige.ch/gcpd/ph01.html> and <http://obswww.unige.ch/gcpd/ph54.html>.
Photometric data for the observed stars Id Identification number --- Name EXOSAT name (Catalogue <VI/43>) --- ObsSeason Code for the observing season number=1 The code is composed by the initial of the month followed by the two last numbers of the year. --- n_ObsSeason When "o": data from Paper I: Cutispoto G. et al 1991 --- Vmax V magnitude at maximum luminosity mag U-B U-B color index mag B-V B-V color index mag V-Rc V-R_c_ color index (Cousins) mag V-Ic V-I_c_ color index (Cousins) mag Qual Quality of the data --- Var Variability flag --- n_Var Uncertainty on variability flag --- Photometric data Id Identification number --- EXOSAT EXOSAT name --- Other Other catalogue number --- Sp Spectral type --- Dist Distance pc n_Dist Uncertainty on distance --- Var Variability flag --- Period Period of variability d n_Period Uncertainty on period of variability --- l_DeltaV Limit flag on amplitude in V-band --- DeltaV Amplitude in the V-band mag Simona Mei CDS 1995 Sep 25 J_A+AS_115_41.xml A CO Survey of Galaxies with the SEST and the 20-m Onsala Telescope J/A+AS/115/439 J/A+AS/115/439 CO survey of galaxies A CO Survey of Galaxies with the SEST and the 20-m Onsala Telescope T Elfhag R S Booth L E B Johansson B Hoeglund A Sandqvist Astron. Astrophys. Suppl. Ser. 115 439 1996 1996A&AS..115..439E Carbon monoxide Galaxies, radio galaxies: ISM radio lines: ISM A large survey of galaxies in the J=1-0 CO line, performed during 1985-1988 using the 15-m SEST and the 20-m millimetre wave telescope of Onsala Space Observatory, is presented. The HPBW of the telescopes are 44" and 33" at 115GHz, respectively. The central positions of 168 galaxies were observed and 101 of these were detected in the CO line. More than 20% of these are new detections. Maps of some of the galaxies are also presented.
Properties of galaxies detected in the CO J=1-0 line Name Galaxy name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Tmb.dV Integrated line intensity [T(mb) x dV] K.km/s e_Tmb.dV Error of line intensity K.km/s RV Radial velocity (LSR) km/s DRV V(heliocentric)-V(LSR) km/s Ref Previous detections (references) number=1 References [Telescope diameter]: 0 - Young et al. (1995) [14 m]; 1 - Solomon & Sage (1988) [14,12 m]; 2 - Young et al. (1989) [ 14 m]; 3 - Braine et al. (1993) [30 m]; 4 - Tinney et al. (1990) [12 m]; 5 - Sanders et al. (1991) [12 m]; 6 - Aalto et al. (1991)[20, 15 m]; 7 - Stark et al. (1987) [7 m]; 8 - Sanders & Mirabel (1985) [12, 14 m]; 9 - Sage (1993) [12 m]; 10 - Mirabel et al. (1990) [15 m]; 11 - Heckman et al. (1989) [12 m]; 12 - Wiklind & Henkel (1989) [30, 20, 15 m]; 13 - Devereux et al. (1994) [45 m]; 14 - Taniguchi et al. (1994) [45 m]; 15 - Jackson et al. (1989) [14 m]; 16 - Tacconi et al. (1991) [15 m]; 17 - Schoeniger & Sofue (1994) [45 m]; 18 - Kenney et al. (1992) [OVRO interferometer]; 19 - Elmegreen & Elmegreen (1982) [11 m]; 20 - Chini et al. (1992) [15, 30 m]; 21 - Stark et al. (1986) [7 m]; 22 - Taniguchi et al. (1990) [45 m]; 23 - Wiklind et al. (1993) [30 m]; 24 - van Driel et al. (1995) [45m]; 25 - Richmond & Knapp (1986) [7 m]; 26 - Sofue (1994) [45 m] ; 27 - Sofue & Nakai (1994) [45 m] --- Mtype Type --- Diam Optical diameter arcmin Diam/beam Optical diameter/Main beam --- Tel Telescope (O=Onsala or S=SEST) --- LogL(CO) CO luminosity K.pc+2.km/s LogL(IR) IR luminosity solLum LogL(B) B luminosity solLum Galaxies searched for CO, with negative results Name Galaxy name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec RV Radial velocity (LSR) km/s Com Comment number=1 + a search was also carried out at a velocity of 2500 km/s ++ searches were also carried out at velocities of 2500, 3500 & 4500km/s --- Tmb RMS[T(mb)] K Mtype Type --- Patricia Bauer CDS 1995 Nov 21 Aa. Sandqvis <sandqvis@astro.su.se> J_A+AS_115_439.xml New proper-motion stars with declination between -5deg and -30deg and right ascension between 0h and 9h J/A+AS/115/481 J/A+AS/115/481 New proper-motion stars -30<Dec<-5, 0<RA<9h New proper-motion stars with declination between -5deg and -30deg and right ascension between 0h and 9h H Wroblewski C Torres Astron. Astrophys. Suppl. Ser. 115 481 1996 1996A&AS..115..481W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/78/231 : Dec<-40, 0<RA<4h30, stars 1 to 144 (Wroblewski+ 1989) J/A+AS/91/129 : Dec<-40, 0<RA<4h30, stars 145 to 521 (Wroblewski+ 1991) J/A+AS/105/179 : Dec<-40, 16<RA<24h, stars 522 to 1069 (Wroblewski+ 1994) J/A+AS/83/317 : LTT stars, Dec<-40, 0<RA<4h30 (Wroblewski+ 1990) J/A+AS/92/449 : LTT stars, Dec<-40, 4h30<RA<16h (Wroblewski+ 1992) J/A+AS/110/27 : LTT stars, Dec<-40, 16<RA<24h (Wroblewski+, 1995) Luyten W.J. 1957, A Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motions Exceeding 0.2 arcsec Annualy (The Lund Press, Minneapolis, Minnesota). Luyten W.J. 1979, LHS Catalogue, University of Minnesota, Minneapolis, Minnesota. (Cat. <I/87>) Proper motions astrometry stars: kinematics Data are given for 494 new stars with proper motion larger than 0.15arcsec/year found on 21 areas covering 25 square degrees each. These are located between -5deg and -30deg in declination and between 0h and 9h in right ascension. Photographic magnitudes range from 9.5 to 19.0. Eight stars have proper motions larger than 0.5arcsec/year, in a magnitude range between 15.5 and 19.0.
Positions and relative proper motions WT Running number --- Loc Localisation (area and number) --- mpg Photographic magnitude, accurate to 0.5mag mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RAh2000 Right Ascension 2000 (hours) h RAm2000 Right Ascension 2000 (minutes) min RAs2000 Right Ascension 2000 (seconds) s DE-2000 Declination 2000 (sign) --- DEd2000 Declination 2000 (degrees) deg DEm2000 Declination 2000 (minutes) arcmin DEs2000 Declination 2000 (seconds) arcsec pm Total proper motion arcsec/yr e_pm Mean error on pm arcsec/yr pmPA Position angle (North to East) of the proper motion in J2000 equinox deg Remark Remarks number=1 4 : when proper-motion is the mean of #4 pairs of plates (*), a : probably companion of LTT 10 b : probably companion of LTT 28 c : probably companion of LTT 331 d : probably companion of LTT 399 e : probably companion of LTT 490 f : probably companion of LTT 1510 g : probably companion of LTT 1727 h : probably companion of LTT 1752 i : probably companion of SAO 171495 j : probably companion of LTT 2634 --- James Marcout, Patricia Bauer CDS 1997 Mar 13 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_115_481.xml Measures and discoveries of visual double stars made with the 50 cm refractor at the Nice Observatory. J/A+AS/115/59 J/A+AS/115/59 Double stars measurements at Nice Obs. Measures and discoveries of visual double stars made with the 50 cm refractor at the Nice Observatory. J C Thorel Astron. Astrophys. Suppl. Ser. 115 59 1996 1996A&AS..115...59T Stars, double and multiple astrometry binaries: visual Measures and discoveries of visual double stars made at the Observatoire de la Cote d'Azur at Nice, between 1988 and 1994, with the 50 cm refractor equipped with a filar micrometer and electronic recording device. The programs proposed by J. Dommanget involve the complement of the C.C.D.M. (resolving problems of identification of double stars and of coherency in the Index) and the INput CAtalog Hipparcos (resolution of ambiguities on the binarity and on the position of certain double stars which have seldom or never been observed again from the epoch or their discovery)
Measurements Name Name of the couple or of the system --- RAh1 Right ascension (1900) h RAdm1 Right ascension (1900) 0.1min DE-1 Declination sign --- DEd1 Declination (1900) deg DEs1 Declination (1900) arcsec RAh2 Right ascension (2000) h RAdm2 Right ascension (2000) 0.1min DE-2 Declination sign --- DEh2 Declination (2000) deg DEs2 Declination (2000) arcsec Mag(1) Magnitude of the first component mag n_Mag(1) When 'V'= variable --- Mag(2) Magnitude of the second component mag Date Date of observation (Universal Time) yr Theta Position angle deg n_Theta See note number=1 n = nuages (clouds) v = vue simple (single) p = vue, pas mesure (seen, not measured) --- Rho Separation arcsec Nights Number of nights of observation --- ADS Number in the Aitken catalogue --- BD Number in Bonner Durchmusterung --- HIC Number of entry in Hipparcos Input Catalog --- Notes Notes (in French) number=2 1 - COU 349 AB = AGK3 +24deg55 2 - MLR 287 AB - Anonyme , precede la BD+69deg29 de 24 secondes et la meme declinaison 3 - MLB 379 ABC = LAM 1 ABC - Systeme triple decouvert par J. von LAMONT en 1836 (Index) , W. Milburn le mesure en 1925 (ADS) et le voit inverse 4 - JCT 2 AB - Decouverte par l'auteur le 18 septembre 1992. C'est le dedoublement de la composante A du systeme multiple STI 237 (circulaire UAI no 118, octobre 1992) 5 - STI 237 EF = HJ 1083 AB 6 - MLR 388 AB - Anonyme , suit la BD+74deg128 de 2 minutes 10 secondes et 12' au Nord 7 - JCT 1 AB - Decouverte par l'auteur le 29 decembre 1991 et premiere mesure effectuee le 31 decembre 1991. Anonyme , precede STF 372 de 17 secondes et 5' au Nord 8 - STF 372 AB = BD+45deg739 et non BD+45deg738 (erreur dans l'ADS et le HIC). Sur le ciel nous voyons tres bien une etoile brillante (BD+45deg738) au Nord de STF (BD+45deg739). Les coordonnees sont: 03 12.7 N 45 35 (1900) et 03 19.3 N 45 57 (2000) 9 - FOX 11 AB = POU 1883 BA - A. POURTEAU decouvre ce couple en 1901 (catalogue des etoile doubles de la zone 24deg de la carte photographique du ciel - POURTEAU 1933). FOX la measure en 1914 (ADS) et decouvre la composante C 10 - JCT 3 AB - Decouverte par l'auteur le 16 decembre 1992 et observee a nouveau le 25 decembre 1994, c'est le dedoublement de la composante A de HO 524 (ADS 6696) . Lors de sa prospection de recherche d'etoiles doubles P. COUTEAU a vu cette composante simple le 27 novembre 1972 (Cahiers d'observations) 11 - A 1103 AB = AG - Recensee dans le catalogue de Leipzig en 1894 , J. MILLER le mesure en 1903 (ADS) et R.G. AITKEN en 1905 (Lick Observatory Bulletin vol. IV -1905-1908, no 93) 12 - BAL 1172 A = RST 5386 - Decouverte par BAILLAUD en 1894 , R.A. ROSSITER la mesure en 1946 (WDS) 13 - A 15 AB = HW 13 - Decouverte en 1884 par H.C. WILSON (ADS), R.G. AITKEN la mesure en 1899. (Astronomische Nachrichten, Band 152, no 3636, p. 61, 1900) 14 - BAL 237 AB = RST 4539 - Decouverte par BAILLAUD en 1902, R.A. ROSSITER la mesure en 1938 (WDS) 15 - HLM 9 AB - Decouverte par E. HOLMES, les mesures sont du Reverend T.E.H. ESPIN en 1922 (ADS), de A. ALI en 1930 et de S.C. BARTON en 1942 (WDS) 16 - PTT -- A - Decouverte en 1916 par E. PETTITT (ADS), elle est vue "simple" par W.D. Heintz en 1962. (Journal des Observateurs vol. 46, p. 1, 1963). PETTITT l'a peut-etre confondue avec STF 2622 situee un peu plus au Nord et dont les parametres sont semblables 17 - COU 226 AB - Vue, mais pas mesuree cause d'une image trop instable 18 - COU 135 AB = Paris +22deg 21h 44 no 428/427. --- Simona Mei CDS 1995 Jul 05 J_A+AS_115_59.xml Optical astrometry of Benchmark radio sources. III. Positions of 35 southern extragalactic radio sources with respect to the International Reference Stars catalogue. J/A+AS/115/75 J/A+AS/115/75 Optical astrometry of Benchmark radio sources. III Optical astrometry of Benchmark radio sources. III. Positions of 35 southern extragalactic radio sources with respect to the International Reference Stars catalogue. E Costa P Loyola Astron. Astrophys. Suppl. Ser. 115 75 1996 1996A&AS..115...75C QSOs Radio sources astrometry quasars: individual (Q0523-570) radio continuum: stars reference systems Optical positions, relative to the International Reference Stars catalogue (IRS), and therefore in the system of the FK5, have been obtained for the optical counterparts of 35 extragalactic radio sources south of {delta}~+3deg. Many of these sources are being considered as possible Benchmark objects for the establishment of a quasi-inertial unified radio/optical reference frame. Precision levels better than 0.2" in both coordinates were achieved. A comparison with VLBI radio positions available for these sources is presented. We give evidence for a possible offset in RA between the radio and optical reference frames.
Optical positions in the FK5 system of 35 extragalactic radio sources IAU IAU designation of the source --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s e_RAs Error on right ascension: {sigma}({alpha}cos{delta}) number=1 Determined as described in Costa and Loyola 1992 arcsec DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec e_DEs Error on declination: {sigma}(cos{delta})(1) arcsec Date Epoch of observation "DD/MM/YY" Notes Notes --- Comparison in the FK5 system with the radio positions of the NRL/USNO Survey IAU IAU designation of the source number= Table 2 (continued): ------------------------------------------ Mean residual -0.24 0.04 Sigma 0.27 0.22 Standard error 0.07 0.06 Nx of common objects 15 ------------------------------------------ --- DeltaRA Difference with the VLBI radio position from the NRL/USNO Survey (Fey et al. 1994); NRL-CL (CL=this paper); Delta {alpha} cos {delta} number= Table 2 (continued): ------------------------------------------ Mean residual -0.24 0.04 Sigma 0.27 0.22 Standard error 0.07 0.06 Nx of common objects 15 ------------------------------------------ arcsec DeltaDE Difference with the VLBI radio position from the NRL/USNO Survey (Fey et al. 1994); NRL-CL (CL=this paper); Delta {delta} number= Table 2 (continued): ------------------------------------------ Mean residual -0.24 0.04 Sigma 0.27 0.22 Standard error 0.07 0.06 Nx of common objects 15 ------------------------------------------ arcsec Simona Mei CDS 1995 Sep 06 J_A+AS_115_75.xml A CS(2-1) survey of IRAS point sources with color characteristics of ultra-compact H II regions J/A+AS/115/81 J/A+AS/115/81 A CS A CS(2-1) survey of IRAS point sources with color characteristics of ultra-compact H II regions L Bronfman L -A Nyman J May Astron. Astrophys. Suppl. Ser. 115 81 1996 1996A&AS..115...81B H II regions Infrared sources Radio lines Galaxy: structure HII regions infrared: ISM ISM: clouds ISM: molecules radio lines: molecular We have made a complete survey of the CS(2-1) emission toward IRAS point sources in the galactic plane. The sources observed were selected according to their far infrared (FIR) colors, which are characteristic of UC HII regions. They have 25{mu}m/12{mu}m flux ratios larger than 3.7 and 60{mu}m/12{mu}m flux ratios larger than 19.3. The survey covered a region from b=-2deg to b=2deg from l=300deg to l=0deg and from l=0deg to l=60deg, and from b=-4deg to b=4deg elsewhere. We detected 843 sources out of 1427 sources observed. The distributions of detected and undetected sources in a FIR color-color diagram show some differences, suggesting that more than one type of object is present in our observed sample.
CS(2-1) survey of UC HII regions GLONG Galactic longitude deg GLAT Galactic latitude deg VLSR Mean local standard rest velocity km/s Tmb Line intensity K DeltaV Line width km/s IRAS IRAS source identification --- Telescope Telescope used for the observation number=1 S= SEST (Swedish-ESO Submillimiter Telescope) O= OSO (Onsala Space Observatory) *= respective spectrum is of poor quality --- Simona Mei CDS 1995 Sep 07 J_A+AS_115_81.xml Astrometry with the Digitized Sky Survey. Positions of 790 AGNs J/A+AS/115/97 J/A+AS/115/97 Positions of 790 AGNs Astrometry with the Digitized Sky Survey. Positions of 790 AGNs M -P Veron-Cetty P Veron Astron. Astrophys. Suppl. Ser. 115 97 1996 1996A&AS..115...97V Active gal. nuclei QSOs astrometry galaxies: active quasars: general From the measurement on the Digitized Sky Survey of the optical position of 153 QSOs with an accurate VLBI position, we have determined that the r.m.s. uncertainties of these measurements is about 0.6 arcsec in both coordinates over the whole sky, except for objects located near the edge of the plates. We have measured the optical position of 790 AGNs (or AGNs candidates). For many of these objects, the accuracy of the published optical position was one arcminute or worst.
Optical J2000 position for 153 QSOs with absolute VLBI position. Name Name of the source --- RAh Right Ascension J2000 (hours) (optical) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec dRA optical - radio right ascension arcsec dDE optical - radio declination arcsec Xpos Rectangular coordinate toward East measured from the centre of the plate cm Ypos Rectangular coordinate toward North measured from the centre of the plate cm Optical position for 790 AGNs (and AGN candidates) Name Name of the source --- RAh1950 Right Ascension B1950 (hours) h RAm1950 Right Ascension B1950 (minutes) min RAs1950 Right Ascension B1950 (seconds) s DE-1950 Declination B1950 (sign) --- DEd1950 Declination B1950 (degrees) deg DEm1950 Declination B1950 (minutes) arcmin DEs1950 Declination B1950 (seconds) arcsec RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Xpos Rectangular coordinate toward East measured from the centre of the plate cm Ypos Rectangular coordinate toward North measured from the centre of the plate cm FC Reference for the finding chart (see file "refs") --- Note Remarks number=1 C indicates that the position has been measured with the cursor rather than with a Gaussian fitting routine. * indicates that the object is located near the edge of the plate ( |X| or |Y| > 14.7 cm ) 1 double sep. 3" 2 weak object at 5.0" N 3 extended 4 double sep. 4" 5 double object 6 weak object at 3.8" 7 object at 6.0" N 8 weak object at 3.5" NW --- References for table2 FC Reference as in table2, blank for continuation --- Text Text of reference --- Francois Ochsenbein CDS 1995 Jul 13 Mira Veron <mira@obshpx.obs-hp.fr> J_A+AS_115_97.xml SEST observations of extragalactic radio sources at 3 mm and 1.3 mm J/A+AS/116/157 J/A+AS/116/157 SEST obs. of extragalactic radiosources SEST observations of extragalactic radio sources at 3 mm and 1.3 mm M Tornikoski E Valtaoja H Terasranta K Karlamaa M Lainela K Nilsson J Kotilainen S Laine A Lahteenmaki L B G Knee L C L Botti Astron. Astrophys. Suppl. Ser. 116 157 1996 1996A&AS..116..157T Galaxies, radio Radio sources galaxies: active quasars: general radio continuum: galaxies telescopes Flux densities of 155 extragalactic radio sources observed with the SEST telescope at 3mm and 1.3mm are presented. The observations were performed from October 1987 to June 1994. In addition to the flux density tables we have plotted the flux density curves for some of the most frequently observed sources.
Flux density data for 155 extragalactic radio sources observed with the SEST-telescope at 3 mm and 1.3 mm Name Radiosource name --- Lambda Wavelength (3mm or 1.3mm) mm Date Observation date "DD/MM/YY" OBSh Observation time (hours) h OBSm Observation time (minutes) min S Flux density at Lambda Jy e_S rms uncertainty on flux density Jy Patricia Bauer CDS 1996 Jan 12 J_A+AS_116_157.xml Global H I profiles of spiral galaxies J/A+AS/116/15 J/A+AS/116/15 Observation of 57 spirals Global H I profiles of spiral galaxies J J Kamphuis D Sijbring T S Van Albada Astron. Astrophys. Suppl. Ser. 116 15 1996 1996A&AS..116...15K VII/155 : RC3 Catalogue (de Vaucouleurs et al., 1991) Galaxies, radio catalogs galaxies: ISM galaxies: spiral radio lines: galaxies In this paper we present short H I synthesis observations of 57 galaxies without H I information in the RC3. These are a by-product of a large survey with the WSRT of the neutral hydrogen gas in spiral and irregular galaxies. Global profiles and related quantities are given for the 42 detected galaxies and upper limits for the remaining 15. A number of galaxies have low values of H I mass-to-blue luminosity ratio.
Result of short WSRT observations for 57 UGC galaxies UGC UGC number (Catalogue <VII/26>) --- NGC NGC or IC number --- Freq Spectral bandwidth of the observation. MHz dV Hanning tapered velocity resolution km/s MType Morphological type as given in the RC3 --- i Inclination of the galaxy deg d Distance Mpc D25 Angular optical diameter (log) at the blue isophote 25mag/arcsec2 as given in the RC3 0.1arcmin B0T Apparent blue magnitude as given in the RC3 mag W50 Observed width of the global profile at the 50% level of the flux density peak. No widths are given for galaxies with poor global profiles. km/s e_W50 rms uncertainty on W50 km/s W50i Width of the global profile at a level of 50% of the flux density peak km/s Vopt Optical heliocentric systemic velocity km/s VHI 21-cm heliocentric systemic velocity derived from the global HI profile km/s e_VHI rms uncertainty on VHI km/s FI Integral of the global profile Jy.km/s l_MHI Limit flag on MHI --- MHI Total HI mass 10+9solMass l_M/L Limit flag on M/L --- M/L Total HI mass to bluer luminosity ratio solMass/solLum Note Notes on individual galaxies number=1 a. (UGC 1034) Possibly also HI emission at the edge of the spectral band. b. (UGC 2067) The observed global profile is possibly that of the companion UGC 2065, a face-on Smb. galaxy at 2.5 arcmin from UGC 2067. c. W_20_ has been determined for four galaxies: UGC 3165: 141 (+/-5) km/s; UGC 4825: 319(+/-8)km/s; UGC 7329: 236(+/-17)km/s; UGC 11466: 251(+/-7)km/s d. (UGC 4271) Arp 9. e. (UGC 9852) Arp 90. --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 Jan 18 J_A+AS_116_15.xml A 12CO(1-0) survey of spiral galaxies in the region of the Coma supercluster. J/A+AS/116/193 J/A+AS/116/193 CO survey of spirals in Coma supercluster A 12CO(1-0) survey of spiral galaxies in the region of the Coma supercluster. F Casoli J Dickey I Kazes A Boselli G Gavazzi K Jore Astron. Astrophys. Suppl. Ser. 116 193 1996 1996A&AS..116..193C Galaxies, radio Radio lines galaxies: clusters: individual (Coma cluster) galaxies: ISM radio lines: galaxies We present observations of the ^12^CO(J=1-0) line at 2.6mm of 65 galaxies located in the Coma supercluster region: 33 actually belong to the Coma supercluster while 32 are either foreground or background objects. These data have been obtained using the NRAO 12m telescope at Kitt Peak (United States), and for four galaxies, using the IRAM 30m telescope at Pico Veleta (Spain). Out of these 65 galaxies, 54 had never been observed in the CO(1-0) line; 49 have been detected by us, of which 37 are new detections. We give molecular gas masses deduced from the CO line integrated intensities, and upper limits for the 16 undetected objects, computed with a Galactic conversion factor N(H_2_)=2.3x10^20^I(CO) and H_0_=75km/s/Mpc.
General data on the surveyed galaxies Name Galaxy name from the General Catalogue of Galaxies and Clusters of Galaxies (Zwicky et al., 1961-1968) --- PCG Name of the galaxy in the Principal Catalog of Galaxies (Paturel et al., 1989) --- RAh Right ascension 1950 (hours) h RAm Right ascension 1950 (minutes) min RAs Right ascension 1950 (seconds) s DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RVel Heliocentric velocity centering of the observations km/s Agg Aggregation parameter --- Dist distance to the source in Mpc Mpc Mtype morphological type from the LEDA database (Lyon-Meudon Extragalactic DAtabase) --- Tel telescope used (KP = NRAO 12m, IR = IRAM 30m) --- OtherNames some other names --- CO(1-0) data Name Galaxy name as in Table 1 --- IntTime Total integration time min l_Area Limit flag on Area --- Area Area of the CO(1-0) K.km/s e_Area rms uncertainty on Area K.km/s Vel Velocity of the CO line km/s e_Vel rms uncertainty on Vel km/s CO CO linewidth km/s e_CO rms uncertainty on CO linewidth km/s Noise rms noise mK l_MH2 Limit flag for mass of molecular hydrogen --- MH2 Mass of molecular hydrogen computed with the distance given in Table 1 and a conversion factor of 2.3 10^20 10+9solMass Patricia Bauer CDS 1996 Jan 05 F. Casoli, <Fabienne.Casoli@obspm.fr> J_A+AS_116_193.xml Monitoring MWC560=V694 Mon in 1990-1995. I. Conventional and high-speed UBV photometry J/A+AS/116/1 J/A+AS/116/1 UBV photometry of MWC560 Monitoring MWC560=V694 Mon in 1990-1995. I. Conventional and high-speed UBV photometry T Tomov D Kolev M Ivanov A Antov A Jones M Mikolajewski A Lepardo R Passuello S Saccavino G Sostero T Valentinuzzi Y Bellas-Velidis A Dapergolas U Munari Astron. Astrophys. Suppl. Ser. 116 1 1996 1996A&AS..116....1T J/A+AS/122/43 : V694 Mon plate spectra (Tomov+ 1997) Photometry, UBV Stars, variable binaries: close binaries: symbiotic stars: individual (MWC 560) stars: magnetic fields stars: mass-loss We present results of an extensive photometric monitoring campaign of the peculiar emission star MWC 560 that covers the range 1990-1995. The time interval corresponds to the length of the proposed orbital period of this highly peculiar binary, which attracted considerable interest in January-April 1990, when absorption components, shifted by -6000km/s from corresponding emission lines, were observed. Here we present photometric data secured during: 113 nights of conventional UBV photoelectric photometry, 45 nights of high speed UBV photoelectric photometry to study the flickering activity, and 682 visual photometric estimates. MWC 560 has experienced a decrease in magnitude since the bright (V=9.2mag) phase in 1990. After the minimum reached in May 1994 (V=10.7mag), the star is currently increasing slowly in brightness. The decrease has been accompanied in all bands by large fluctuations superimposed on the mean trend. The B-V colour has shown a steady increase by 0.0.33mag/yr. U-B has remained stable at -0.07mag since late 1990. In all the observing nights devoted to high speed photometry we observed flickering activity in MWC 560. The data show that the flickering amplitude {DELTA}U increases with the decrease of the U magnitude. Quasi-periodic variations have always been detected. A period of ~70min has been observed in ~13 nights which is close to the ~60min quasi-period reported by Michalitsianos et al. (1993). However, no coherent variability is traceable throughout the whole set of flickering data.
MWC 560 V694 Mon 07 23 25.9 -07 38 03
UBV photoelectric photometry JD Date of the observation d Vmag Star's magnitude in V band mag u_Vmag Uncertainty flag on Vmag --- B-V B-V colour mag u_B-V Uncertainty flag on B-V --- U-B U-B colour mag u_U-B Uncertainty flag on U-B --- o_Vmag Number of independent measurements --- Obs Identification of the Observatory number=1 The observatories are: Roz = Bulgarian National Astronomical Observatory Rozhen, Bel = Belogradchik Astronomical Observatory, Kry = Kryoneri Observatory in Greece, Tor = Torun Observatory in Poland, Ols = Olsztyn Observatory in Poland, Suh = Mt. Suhora Observatory in Poland, Rem = Remanzacco Observatory of the Assoziazione Friulana di Astronomia e Meteorologia (Italy). --- Visual brightness estimates of MWC560 from Nelson (New Zealand) JD Date of the observation d Vmag Visual brightness estimates mag Patricia Bauer CDS 1996 Jan 15 T. Tomov, <rozhen@tempus.tu-plovdiv.bg> J_A+AS_116_1.xml Structure and kinematics of galaxy clusters I. The redshift catalogue J/A+AS/116/203 J/A+AS/116/203 The redshift catalogue for galaxy clusters Structure and kinematics of galaxy clusters I. The redshift catalogue P Stein Astron. Astrophys. Suppl. Ser. 116 203 1996 1996A&AS..116..203S Clusters, galaxy Redshifts catalogs galaxies: clusters: general galaxies: distances and redshifts An extensive redshift survey has been conducted on a sample of 15 nearby (0.01<~z<~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.
Redshifts and types inside clusters Redshifts and types outside clusters Name Cluster or field name: --- Seq Sequential identification of objects --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec HRVem Heliocentric radial velocity from emission lines km/s e_HRVem Error on radial velocity from emission lines km/s HRVabs Heliocentric radial velocity from absorption lines (cross-correlation) km/s e_HRVabs Error on radial velocity from absorption lines km/s HRV Combined heliocentric radial velocity km/s e_HRV Error on radial velocity km/s Nem Number of emission lines from which `HRVem' was determined --- MType Morphological class for the galaxy --- r_MType Source number=1 Morphological types were taken either from the literature or determined directly on ESO-survey plates --- Simona Mei CDS 1995 Sep 07 J_A+AS_116_203.xml Star counts in southern dark clouds: Corona Australis and Lupus J/A+AS/116/21 J/A+AS/116/21 Extinction toward CrA and Lup Star counts in southern dark clouds: Corona Australis and Lupus C M Andreazza J W S Vilas-Boas Astron. Astrophys. Suppl. Ser. 116 21 1996 1996A&AS..116...21A Extinction dust, extinction ISM: clouds ISM: individual (CrA cloud, Lup cloud) ISM: magnetic fields Star counts technique is used towards southern dark globular filaments situated in the cloud complexes of Corona Australis and Lupus. Tables and maps of the distribution of visual extinction are presented for each filament. Lower limit masses for the filaments and condensations have been estimated and the central coordinates of the condensations are also given. R CrA is the most active star forming region among the filaments studied in this work whereas Lupus 1, with almost the same lower limit of mass, has only a few T Tauri stars and just one young embedded object. The distribution of direction of the magnetic field in the condensations of Lupus, suggests that the condensation morphologies does not have any apparent relation with the magnetic field orientation.
Visual extinction dist. toward Corona Australis Visual extinction distribution toward Lupus 1 Visual extinction distribution toward Lupus 2 Visual extinction distribution toward Lupus 3 Visual extinction distribution toward Lupus 4 I Index of the data column in right ascension, the offset for the point I in right ascension from the (0, 0) position is I*2.25arcmin --- J Index of the data column in declination, the offset for the point J in declination from the (0, 0) position is J*2.25 arcmin --- Ext Visual extinction, value of the element I, J of the matrix which correspond to a square of 2.25 arcmin mag n_Ext Lower limit to the visual extinction --- Patricia Bauer CDS 1996 Jan 22 J_A+AS_116_21.xml A library of H band stellar spectra for stellar population analysis purpose J/A+AS/116/239 J/A+AS/116/239 H band stellar spectra A library of H band stellar spectra for stellar population analysis purpose R Dallier C Boisson M Joly Astron. Astrophys. Suppl. Ser. 116 239 1996 1996A&AS..116..239D Spectra, infrared atlases infrared: stars line: identification stars: classification stars: fundamental parameters stars: late-type A sample of 37 stars of luminosity classes I, III, V, including few SMR stars observed in the H band with a medium resolution (R=1500-2000) is presented. This sample of flux calibrated spectra is intended to widen existing stellar libraries. Observations were conducted with the ISIS spectrograph at CFHT and with IRSPEC at ESO-NTT. The wavelength range covers 1.573-1.646 micron at NTT (R=1490 at 1.60micron) and 1.578-1.642 micron at CFHT (R=2000 at 1.60micron). Spectra are in relative fluxes, F(lambda), normalized to 1 in the range 1.59290-1.59506 micron. In the few cases where a star was observed both with ISIS and IRSPEC, both spectra are given. So the number of files is in fact 41 concerning 37 stars.
Observed stars n_Name A '*' indicates stars used for photometric standards --- Name Star name --- Sp Spectral type --- Tel Telescope --- Spect Spectrocopic observation band --- [Fe/H] Metallicity --- Ref Reference number=1 BG90 : Barbuy & Grenon, 1990 C&92 : Cayrel et al., 1992, catalog <III/165> McW90 : McWilliam, 1990 T91 : Taylor, 1991 Z91 : Zhou, 1991 --- Equivalent widths Obs Type of observations, ISIS or IRSP (IRSPEC) --- Sp spectral type --- n_Sp Note; SMR for Super Metal Rich mp for metal poor --- Names Stars involved --- CO1.58 CO1.58 equivalent width (1.5755-1.5805um) 0.1nm SiI+FeI SiI+FeI equivalent width (1.5805-1.5854um) 0.1nm FeI1.58 FeI1.58 equivalent width (1.5854-1.5872um) 0.1nm SiI1.59 SiI1.59 equivalent width (1.5872-1.5903) 0.1nm FeI1.591 FeI1.591 equivalent width (1.5903-1.5914) 0.1nm FeI1.592 FeI1.592 equivalent width (1.5914-1.5934) 0.1nm SiI1.60 SiI1.60 equivalent width (1.5934-1.5973) 0.1nm CO1.60 CO1.60 equivalent width (1.5973-1.5996) 0.1nm FeI1.60 FeI1.60 equivalent width (1.5996-1.6030) 0.1nm OH1.60 OH1.60 equivalent width (1.6030-1.6058) 0.1nm SiI+FeIb SiI+FeI equivalent width (1.6058-1.6085) 0.1nm SiI+FeIc SiI+FeI equivalent width (1.6085-1.6143) 0.1nm FeI+CaI FeI+CaI equivalent width (1.6143-1.6171) 0.1nm CO1.62 CO1.62 equivalent width (1.6171-1.6190) 0.1nm CaI1.62 CaI1.62 equivalent width (1.6190-1.6225) 0.1nm FeI+OH FeI+OH equivalent width (1.6225-1.6266) 0.1nm FeI+1.629 FeI+1.629 equivalent width (1.6266-1.6296) 0.1nm FeI1.63 FeI1.63 equivalent width (1.6296-1.6343) 0.1nm u_FeI1.63 Uncertainty flag on FeI1.63 --- NiI+SiI NiI+SiI equivalent width (1.6343-1.6387) 0.1nm u_NiI+SiI Uncertainty flag on NiI+SiI --- Br14+HeI Br14+HeI equivalent width (1.5855-1.5915) number=1 Only for OB stars 0.1nm HeI HeI equivalent width (1.6062-1.6090) number=1 Only for OB stars 0.1nm Br13 Br13 equivalent width (1.6090-1.6140) number=1 Only for OB stars 0.1nm table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 bs788.fit BS788 ISIS spectrum bs1112.fit BS1112 ISIS spectrum bs1123.fit BS1123 ISIS spectrum bs1790.fit BS1790 ISIS spectrum bs2456.fit BS2456 ISIS spectrum bs2764.fit BS2764 ISIS spectrum bs3170.fit BS3170 ISIS spectrum bs3364.fit BS3364 ISIS spectrum bs3459.fit BS3459 ISIS spectrum bs3903.fit BS3903 ISIS spectrum bs4127.fit BS4127 ISIS spectrum bs4133.fit BS4133 ISIS spectrum bs4174.fit BS4174 IRSPEC spectrum bs4456.fit BS4456 ISIS spectrum bs4550.fit BS4550 ISIS spectrum bs4590.fit BS4590 ISIS spectrum bs4638.fit BS4638 IRSPEC spectrum bs4695a.fit BS4695 IRSPEC spectrum bs4695b.fit BS4695 ISIS spectrum bs4883.fit BS4883 ISIS spectrum bs4902a.fit BS4902 IRSPEC spectrum bs4902b.fit BS4902 ISIS spectrum bs4983.fit BS4983 ISIS spectrum bs5020a.fit BS5020 IRSPEC spectrum bs5020b.fit BS5020 ISIS spectrum bs5056.fit BS5056 ISIS spectrum bs5315.fit BS5315 ISIS spectrum bs5645.fit BS5645 IRSPEC spectrum bs5824.fit BS5824 & BS6973 IRSPEC spectrum gl382a.fit GL382 IRSPEC spectrum gl382b.fit GL382 ISIS spectrum hd93800a.fit HD93800 IRSPEC spectrum hd93800b.fit HD93800 ISIS spectrum hd109655.fit HD109655 & BS2731 ISIS spectrum hd111180.fit HD111180 ISIS spectrum hd112758.fit HD112758 ISIS spectrum hd115404.fit HD115404 ISIS spectrum hd130871.fit HD130871 IRSPEC spectrum hd157881.fit HD157881 IRSPEC spectrum hd160691.fit HD160691 IRSPEC spectrum hd175674.fit HD175674 IRSPEC spectrum Patricia Bauer CDS 1996 Jan 12 C. Boisson, <boisson@gin.obspm.fr> J_A+AS_116_239.xml Long- and short-term variability in O-star winds I. Time series of UV spectra for 10 bright O stars. J/A+AS/116/257 J/A+AS/116/257 Variability in O-stars wind Long- and short-term variability in O-star winds I. Time series of UV spectra for 10 bright O stars. L Kaper H F Henrichs J S Nichols L C Snoek H Volten G A A Zwarthoed Astron. Astrophys. Suppl. Ser. 116 257 1996 1996A&AS..116..257K Spectra, ultraviolet Stars, early-type stars: early-type stars: mass-loss ultraviolet: stars The tables below list the Log of IUE observations incorporated in the paper. The table number corresponds to the figure number in the paper. The involved O star and the observing period are mentioned in the table header.
IUE observations Figno Figure number in the paper --- Date Observation date "DD/MM/YY" Seq Sequence number --- Ident Identification number of the observation obtained with the Short Wavelength Prime camera on IUE --- ObsH Start time of the observation (hour) h ObsM Start time of the observation (min) min ExpM Exposure time (min) min ExpS Exposure time (sec) s HJD Julian Day at mid-exposure d Patricia Bauer CDS 1996 Jan 04 J_A+AS_116_257.xml Stark broadening of Xe II lines. J/A+AS/116/359 J/A+AS/116/359 Xe II lines Stark broadening Stark broadening of Xe II lines. L C Popovic M S Dimitrijevic Astron. Astrophys. Suppl. Ser. 116 359 1996 1996A&AS..116..359P VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/117/127 : Stark broadening of solar MgI lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines (1) Nick K. P., Helbig, 1986, Phys. Scr. 33, 55 (2) Di Rocco H. O., 1990b, Il Nuovo Cimento 12D, 1485 (3) Gigosos M. A., Mar S., Perez C. and I. de la Rosa, 1994, Phys. Rev. E49, 1575 (4) Lesage A., Miller M. H., Richou J., Bach T., 1981, in Spectral Line Shapes, Ed. B. Wende, W. de Gruyter, Berlin, New York, p. 257 (5) Lesage A., Abadie D., Miller M. H., 1989, Phys. Rev. A 40, 1367 (6) Miller M. H., Lesage A., Abadie D., 1981, Phys. Rev. A 25, 2064 (7) Bertuccelli D., Bertuccelli G., Di Rocco H. O., 1991, Phys. Scr. 43, 469 (8) Richou J., Manola S., Lebrun J. L., Lesage A, 1984, Phys. Rev. A29, 3181 (9) Vitel Y., Skowronek M., 1987, J. Phys. B 20, 6493 (10) Konjevi'c N., Uzelac N. I., 1990, JQSRT 44, 61 (11) Manola et al. 1988, Phys. Rev. A38, 5742 -------------------------------------------------------------------------------- Atomic physics atomic data plasmas stars: chemically peculiar We present here Stark widths and shifts for 20 Xe II multiplets which are of interest for laboratory plasma research as well as for the analysis of Hg-Mn stars spectra. For calculations the modified semiempirical approach was used. The obtained results are compared with the available experimental data.
*Stark full widths and shifts of Xe II lines Trans Transition --- Lam Wavelength nm T Temperature K W Stark width nm d Stark shift nm Comparison of measured and theoretical values for Stark widths and shifts Trans Transition --- Lam Wavelength nm T Temperature 1000K Wm Measured Stark width nm l_dm Limit flag on dm --- dm Measured Stark shift nm Wm/Wth Measured versus theoretical Stark width --- dm/dth Measured versus theoretical Stark shift --- n_dm/dth Note on dm/dth number=1 When *, the measured and the calculated values of Stark shift have different sign --- Ref References --- table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 Patricia Bauer CDS 1996 Jan 16 J_A+AS_116_359.xml VRI photometry of stars in the fields of 12 BL Lacertae objects J/A+AS/116/403 J/A+AS/116/403 VRI photometry of stars in 12 BL Lac objects VRI photometry of stars in the fields of 12 BL Lacertae objects M Fiorucci G Tosti Astron. Astrophys. Suppl. Ser. 116 403 1996 1996A&AS..116..403F BL Lac objects Photometry, VRI BL Lacertae objects: general We present VR_cI_c Johnson-Cousins magnitudes of field comparison stars for twelve BL Lacertae objects belonging to the more large sample of blazars which is monitored at Perugia Astronomical Observatory. These comparison stars can be used in the long-term CCD photometric monitoring of BL Lac objects aimed to understand the characteristics of their variability. Finding charts for all of these comparison sequences are also included in this paper. For a description of the (RI)c photometric system, see e.g. the General Catalog of Photometric Data <GCPD/54>
VR_c_I_c_ comparison stars in the fields of BL Lacertae objects Name Names of BL Lac objects and respective comparison stars --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Vmag V Johnson magnitude mag e_Vmag Standard deviation on V magnitude mag Rcmag Cousins R magnitude mag e_Rcmag Standard deviation on R_c_ magnitude mag Icmag Cousins I magnitude mag e_Icmag Standard deviation on I_c_ magnitude mag Number Number of nights utilized to calibrate each star --- Refer References for those objects that have previously published photometric sequences in at least one of the VRI filters number=1 Reference numbers are: 1: Bertaud C., Dumortier B., Veron P., et al. (1969), A&A 3, 436. =1969A&A.....3..436B 2: Penston M. V., Wing R. F. (1973), The Observatory 93, 149. =1973Obs....93..149P 3: Craine E. R. (1977), A Handbook of Quasistellar and BL Lacertae Objects, Pachart Publishing House, Tucson. 4: Smith P. S., Balonek T. J., Heckert P. A., et al. (1985), AJ 90, 1184 =1985AJ.....90.1184S 5: Smith P. S., Jannuzi B. T., Elston R. (1991), ApJS 77, 67 =1991ApJS...77...67S 6: Takalo L. O., Sillanpaa A., Nillson K. (1994), A&AS 107, 497 =1994A&AS..107..497T --- Simona Mei CDS 1995 Oct 13 J_A+AS_116_403.xml Morphological classification and structural parameters for early-type galaxies in the Coma cluster. J/A+AS/116/429 J/A+AS/116/429 Classification of Coma early galaxies Morphological classification and structural parameters for early-type galaxies in the Coma cluster. S Andreon E Davoust R Michard J -L Nieto P Poulain Astron. Astrophys. Suppl. Ser. 116 429 1996 1996A&AS..116..429A Galaxy catalogs Morphology Photometry, surface galaxies: clusters: individual (Coma cluster) galaxies: elliptical and lenticular, cD galaxies: fundamental parameters We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.
Observing log Name Abridged GMP or NGC number --- Exp Exposure time s Filt Filter --- Run Observing run --- FWHM Seeing arcsec u_FWHM Uncertainty flag on FWHM --- Sky Sky brightness mag/arcsec+2 Isolim Level of last measured isophote mag/arcsec+2 Notes Notes number=1 (1) presumably absorbed weather; (2) not analysed; (3) spiral; (4) calibration from mean sky brightness; (5) elongated stellar images; (6) calibration uncertain, mean of previous night; (7) near edge of image; (8) very doubtful identity; (9) blended binary; (10) inadequate field; (11) Superimposed on NGC 4889, measured after subtraction of a model image of the cD; (12) underexposed image with bright sky; (13) companion to the W; (14) halo of a very bright star; (15) suspiciously high seeing; (16) very poor seeing; (17) calibrator of KP2225. --- CCD Telescope Bernard Lyot (TBL) subsample photometric parameters and classification CCD CFH subsample photometric parameters and classification KP1608 sample photometric parameters and classification GMPa Number in the abridged version of GMP catalogue <VII/42> --- GMP Number in the unabridged version of GMP catalogue <VII/42> --- Dress Number in Dressler catalogue <VII/174> --- Name NGC, Ic or RB (Rood & Baum 1967) number. --- m_Name Multiplicity index on Name --- Xpos X differential position number=1 X and Y positions in arc seconds relative to the approximate center of the cluster, increasing westwards and northwards respectively. The origin of these coordinates is at RA=12h57.3 Dec=+28d14.4'(1950.0). arcsec Ypos Y differential position number=1 X and Y positions in arc seconds relative to the approximate center of the cluster, increasing westwards and northwards respectively. The origin of these coordinates is at RA=12h57.3 Dec=+28d14.4'(1950.0). arcsec Rmag Asymptotic magnitude in R_c_ mag log(Reff) Effective radius number=10 The units are erroneously indicated as 0.1arcmin in the printed paper. arcsec log(a) Semi-major axis of the effective isophote number=10 The units are erroneously indicated as 0.1arcmin in the printed paper. arcsec SuBr Mean surface brightness inside the effective isophote, in R magnitude mag/arcmin+2 Diskp Photometric evidence for a disk number=2 st: strong; cl: clear; ft: faint; no: none --- b/a Typical axis ratio number=9 Typical value, either its minimum value, if clearly defined, or its value at the effective isophote otherwise --- e4 Typical e4 parameter number=9 Typical value, either its minimum value, if clearly defined, or its value at the effective isophote otherwise % n_e4 Location where the e4 parameter was estimated number=3 ex: at its extremum, re: at the effective isophote, co: if the value is the same at both locations --- b/ae Axis ratio at the envelope, i.e. at the isophote {mu}_r_=24mag/arcsec^2^ --- Ampli Amplitude of isophotal twist in the range of reliable measurements deg Bar Detection of bar number=4 bar: bar seen, bar?: bar suspected, no: no bar seen --- Disk Detection and classification of a disk number=5 emDi: embedded disk, miDi: mixed disk, exDi: extended disk, -?Di: detected but unclassified disk, -no- (no disk seen) --- Spiral Detection of a spiral pattern number=6 spiP: spiral pattern seen, spiP?: spiral pattern suspected, -no-: no spiral pattern seen --- Envelope Classification of an envelope number=7 spH: spheroidal halo, thD: thick disk, exD: extended disk, pec: peculiar envelope, -?-: unclassified envelope --- MType Morphological classification number=8 boE: boxy E, unE: undetermined E, diE: disky E, SA0, SAB0, SB0, Sa, etc., S...: spiral of unknown stage) --- Note Individual notes (see notes file) --- FW sample photometric parameters and classification RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Name NGC, IC or RB (Rood & Baum 1967) number. FW and D from Strom & Strom (1978), anon = anonymous (m_R_<=16.05), supll = anonymous (m_R_> 16.05) --- m_Name Multiplicity index on Name --- Rmag Asymptotic magnitude in R_c_ mag log(Reff) Effective radius number=10 The units are erroneously indicated as 0.1arcmin in the printed paper. arcsec log(a) Semi-major axis of the effective isophote number=10 The units are erroneously indicated as 0.1arcmin in the printed paper. arcsec SuBr Mean surface brightness inside the effective isophote, in R magnitude mag/arcmin+2 Diskp Photometric evidence for a disk number=1 st (strong); cl (clear); ft (faint); no (none) --- b/a Typical axis ratio number=8 Typical value, either its minimum value, if clearly defined, or its value at the effective isophote otherwise --- e4 Typical e4 parameter number=8 Typical value, either its minimum value, if clearly defined, or its value at the effective isophote otherwise % n_e4 Location where the e4 parameter was estimated number=2 ex (at its extremum), re (at the effective isophote), co (if the value is the same at both locations) --- b/ae Axis ratio at the envelope, i.e. at the isophote {mu}_r_=24mag/arcsec^2^ --- Ampli Amplitude of isophotal twist in the range of reliable measurements deg Bar Detection of bar number=3 bar (bar seen), bar? (bar suspected), no (no bar seen) --- Disk Detection and classification of a disk number=4 emDi (embedded disk), miDi (mixed disk), exDi (extended disk), -?Di (detected but unclassified disk), -no- (no disk seen) --- Spiral Detection of a spiral pattern number=5 spiP (spiral pattern seen), spiP? (spiral pattern suspected), -no- (no spiral pattern seen) --- Envelope Classification of an envelope number=6 spH (spheroidal halo), thD (thick disk), exD (extended disk), pec (peculiar envelope), -?- (unclassified envelope) --- MType Morphological classification number=7 boE (boxy E), unE (undetermined E), diE (disky E), SA0, SAB0, SB0, Sa, etc., S... (spiral of unknown stage) --- Note Individual notes (see notes file) --- Patricia Bauer CDS 1996 May 13 J_A+AS_116_429.xml Search for emission-line galaxies towards nearby voids. Observational data J/A+AS/116/43 J/A+AS/116/43 Emission-line galaxies nearby voids. Search for emission-line galaxies towards nearby voids. Observational data C C Popescu U Hopp H J Hagen H Elsaesser Astron. Astrophys. Suppl. Ser. 116 43 1996 1996A&AS..116...43P Galaxy catalogs Redshifts galaxies: distances and redshifts galaxies: irregular large-scale structure of universe surveys We present the observational results of our search for emission-line galaxies (ELG) towards nearby voids. In order to find ELG, we started a survey using the IIIa-J objective prism plates from the Hamburg QSO Survey. The plates are digitized and an automatic procedure was applied to select the candidates. Digitized direct plates were used to determine coordinates and to reject overlaps between spectra. The accuracy of the coordinates is +/-2". A total area of 1248deg^2^ was scanned, distributed in four different regions. All the selected objects were observed with follow-up spectroscopy. We have obtained a final sample of 203 objects, of which 196 are emission-line galaxies, four are galaxies with absorption lines and three are QSOs. Almost half of our objects are newly discovered ones and three quarters of the given redshifts are new. Our sample contains mainly high ionization galaxies and is less sensitive in the detection of low-ionization objects. The apparent magnitudes, as derived from the objective prism plates, range between 15.0<=B<=19.5. The sample is dominated by nearby galaxies, with a peak in the redshift distribution at cz=4500 km/s.
Observational data HS Name of the objects number=1 The name is built with the prefix HS (from Hamburg Survey), followed by the first four digits of the 1950.0 right ascension and declination --- Other Other name --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec z Heliocentric redshift --- Bmag B magnitude mag Bmag2 magnitude form literature, when available mag S Selection criteria number=2 Selection used to select the candidates from the objective prism spectra: E for emission candidate (first priority), and B for blue candidate (second priority) --- Ref Number of the run or code of the reference number=3 Number of the run in which the object was observed (with the prefix o - from observed) or the code of the reference, when the object had available redshift (with the prefix l - from literature). The numbers of the observing runs are the same as listed in Table 2 (see Paper). Codes for the references: A Abell galaxy 1. CG Case Galaxy 53-57, 62-65, 71 CGCG Catalogue of Galaxies and of Cluster of Galaxies 1968, 93. (Catalog <VII/49>) CGPG Catalogue of Selected Compact Galaxies and of Post Eruptive Galaxies 1971, 92. DDO David Dunlap Observatory catalog, van den Bergh 1966, 3. dKM92 de Grijp, Keel, Miley et. al. 1992, 12. G93 Garcia 1993, 11. H Hard X-Ray Sources 42. IRAS Infrared Astronomical Satellite Catalogs 1988. The Point Source Catalog 15. (Catalog <II/125>) IRAS F Infrared Astronomical Satellite Catalogs 1990. The Faint Source Catalog 46. (Catalog <II/156>) KUG Kiso Survey for UV Excess Galaxies 73-76. LGG Lyon Group of Galaxies Catalog 11. MCG Morphological Catalogue of Galaxies 1962, 82-86. MRK Markarian Galaxy 25-40. NPM Lick Northern Proper Motion Program 16. OA-OZ Ohio Source Catalog, 1415 MHz 17, 47, 18, 66, 7, 10, 8, 5, 9, 60 PC Palomar Transit Grism Survey 67. RC2 The Second Reference Catalogue 1976, 79. SMB88 Slezak, Mars, Bijaoi et. al. 1988, 69. SBS Second Byurakan Spectral Sky Survey 41, 70. SP82 Sanduleak and Pesch 1982, 61. UCM Universidad Complutense de Madrid 58, 89, 90 UGC Uppsala General Catalogue of Galaxies 1973, 48. (Catalog <VII/26>) UM University of Michigan 20-24. VV Vorontsov-Velyaminov 1959, 1977, Atlas and Catalog of Interacting Galaxies 81. WAS Wasilewski 1983, 87. XRS Second Catalogue of X-ray Sources 2. Zw Zwicky Compact Galaxy 91. --- Rem Remarks number=4 * -galaxies with only one line detection ** -galaxies with only one line detection but twice observed --- Names Other names --- table4.tex LaTeX version of table4 Patricia Bauer CDS 1996 Jan 22 J_A+AS_116_43.xml The ellipticities of globular clusters in the Andromeda Galaxy. J/A+AS/116/447 J/A+AS/116/447 M31 globulars clusters ellipticities The ellipticities of globular clusters in the Andromeda Galaxy. A Staneva N Spassova V Golev Astron. Astrophys. Suppl. Ser. 116 447 1996 1996A&AS..116..447S Clusters, globular catalogs galaxies: individual (M 31) galaxies: star clusters globular clusters: general The projected ellipticities and orientations of 173 globular clusters in the Andromeda galaxy have been determined by using isodensity contours and 2D Gaussian fitting techniques. A number of B plates taken with the 2m Ritchey-Chretien-coude reflector of the Bulgarian National Astronomical Observatory were digitized and processed for each cluster. The derived ellipticities and orientations are presented in the form of a catalogue. The projected ellipticities of M 31 GCs lie between 0.03/0.24 with mean value {epsilon}=0.086+/-0.038. It may be concluded that the most globular clusters in the Andromeda galaxy are quite spherical. The derived orientations do not show a preference with respect to the center of M 31. Some correlations of the ellipticity with other clusters parameters are discussed. The ellipticities determined in this work are compared with those in other Local Group galaxies
M 31 00 42.7 +41 16
Morphological parameters of M31 globulars Name Clusters' name from Sargent et al.(1977) or Battistini et al.(1987) --- Eps Mean ellipticity --- e_Eps Final rms uncertainty in ellipticity --- PA Position angle of the major axis measured from north toward east deg e_PA Final rms uncertainty in position angle deg Mes Number of measurements --- Method Reduction method (I for isodensity analysis and D for 2D Gaussian) --- a Apparent angular size of the major axis arcsec Comparison of the ellipticities of globulars in M31, Milky Way Galaxy, and Magellanic Clouds Name Name of the galaxy --- Eps Mean ellipticity --- e_Eps rms uncertainty in ellipticity --- Nobj Number of objects in the sample --- l(Eps) Ellipticity range - lower limit --- u(Eps) Ellipticity range - upper limit --- Source Source --- Comparison of the ellipticities with the data of other authors Name Clusters' name after Sargent et al. (1977) --- EpsA1 Annulus A ellipticity, Davoust & Prugniel (1990) --- EpsB1 Annulus B ellipticity, Davoust & Prugniel (1990) --- EpsA2 Annulus A ellipticity, Lupton (1989) --- EpsB2 Annulus B ellipticity, Lupton (1989) --- Eps Ellipticity from this work --- Rad Radius arcsec Patricia Bauer CDS 1996 Feb 08 J_A+AS_116_447.xml Transition probabilities for forbidden lines of Fe III J/A+AS/116/573 J/A+AS/116/573 Transitions for FeIII Transition probabilities for forbidden lines of Fe III P Quinet Astron. Astrophys. Suppl. Ser. 116 573 1996 1996A&AS..116..573Q Atomic physics atomic data Fe III radiative transition probabilities Radiative transition probabilities have been calculated for states within the 3d6 configuration of Fe III. Magnetic dipole (M1) and electric quadrupole (E2) transition probabilities have been obtained using average energies, electrostatic and spin-orbit integrals adjusted so as to fit the observed energy levels. The most important configuration interaction (CI) and relativistic effects were included explicitly in the calculations, using the relativistic Hartree-Fock (HFR) method due to Cowan. The present work represents a refinement of previous monoconfigurational calculations of transition probabilities for forbidden lines of astrophysical interest in Fe III.
Transition probabilities (Aki) for forbidden lines within the 3d6 configuration of Fe III Multiplet Multiplet designation --- J-J' J-J' --- Lambda Predicted wavelengths from observed energy levels number=1 Predicted wavelengths are deduced from the observed energy levels (Ekberg 1993). They are given in air above 200 nm and in vacuum below 200 nm. 0.1nm n_Lambda Comment on the wavelength number=2 c calculated HFR wavelength. --- M1 Transition probabilities for M1 lines s-1 n_M1 Comment on the M1 transition number=3 * Cancellation effects present. --- E2 Transition probabilities for E2 lines s-1 n_E2 Comment on the E2 transition number=3 * Cancellation effects present. --- Francois Ochsenbein CDS 1995 Dec 20 P. Quinet, <pascal@simpa3.univ-rennes1.fr> J_A+AS_116_573.xml Investigation on the region of the open cluster Tr 14 J/A+AS/116/75 J/A+AS/116/75 Region of the open cluster Tr 14 Investigation on the region of the open cluster Tr 14 R A Vazquez G Baume A Feinstein P Prado Astron. Astrophys. Suppl. Ser. 116 75 1996 1996A&AS..116...75V Clusters, open Photometry, UBVRI Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Tr 14) stars: individual (HD 93129AB, HD 93161EW) stars: luminosity function, mass function stars: pre-main sequence We present UBVRI CCD imaging photometry down to approximately V=19mag in the area of the very young open cluster Tr 14. Our results confirm the existence of an anomalous extinction law in the area if it is interpreted in terms of the UBVRI photometry. According to our analysis the cluster distance is d=3100 (V_0_-M_V_=12.50mag) and its age is 1.5+/-.5x10^6^y. We want to draw the attention on stars which, from the observed magnitude-spread at constant color, could be stars in an early stage of evolution. In that case, the observed spread leads to assume that the process of star formation in Tr 14 is continuous whereas, from pre-main sequence evolutionary tracks, a duration of about 5x10^6^y is deduced for it. The computation of the cluster initial mass function reveals a flat slop e even though it still compares to a Salpeter law. At the same time, we found a spatial variation of the cluster IMF, which could be explained by mass segregation in the star formation process. The cluster youth and its compact appearance seem to confirm that it is far from virial equilibrium. The observed tot al cluster mass is around 2000M_{sun}_ and its core contains about 40% of the total.
HD 93129AB 10 43 57.4 -59 32 51 HD 93161EW 10 44 08.87 -59 34 34.7
Observed colors and magnitudes in Tr 14 No Sequence number --- F Identification number in Feinstein, 1983 --- MJ Identification number in Massey & Johnson, 1993 --- CMDE Identification number in Cudworth et al., 1993 --- Xpos X position pix Ypos Y position pix Vmag V magnitude mag u_Vmag uncertainty flag on Vmag number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- B-V B-V color mag u_B-V uncertainty flag on B-V number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- U-B U-B color mag u_U-B uncertainty flag on U-B number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- V-R V-R color mag u_V-R uncertainty flag on V-R number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- V-I V-I color mag u_V-I uncertainty flag on V-I number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- p Membership probability % Rem Remark number=2 m = likely member pm = probable member nm = non-member cs? = star assumed to be in contracting phase ? = uncertain membership. --- Free reddening colors and magnitudes No Sequence number --- V0mag Free reddening V magnitude mag (B-V)0 Free reddening B-V color mag E(B-V) Color excess in B-V mag n_E(B-V) An * indicates that mean color excess was used --- (U-B)0 Free reddening U-B color mag E(U-B) Color excess in U-B mag n_E(U-B) An * indicates that mean color excess was used --- MV V absolute magnitude mag log(Teff) Effective temperature K logL Luminosity solLum logM Present day stellar mass solMass table2.tex LaTeX version of table2 table5.tex LaTeX version of table5 Patricia Bauer CDS 1996 Jan 5 J_A+AS_116_75.xml Planetary nebulae in the Magellanic Clouds : I. Carbon abundances and TypeI PNe J/A+AS/116/95 J/A+AS/116/95 Magellanic Clouds PNe line intensities Planetary nebulae in the Magellanic Clouds : I. Carbon abundances and TypeI PNe P Leisy M Dennefeld Astron. Astrophys. Suppl. Ser. 116 95 1996 1996A&AS..116...95L Magellanic Clouds Planetary nebulae Spectroscopy galaxies: abundances galaxies: evolution Magellanic Clouds planetary nebulae: general We present optical and ultraviolet spectroscopic observations of planetary nebulae (PNe) in the Large (LMC) and the Small Magellanic Clouds (SMC). For the visible spectra with highest S/N, line intensities have been measured to a few tenths of a percent of H_{beta}_. UV spectra are used for the determination of carbon abundances. This paper discusses the CNO cycle and its implications. We show that the CN or ON cycles are more effective with lower initial metallicities and are always complete for typeI nebulae. The latter cannot easily be distinguished from non-type I PNe on the basis of N or He abundance alone, as continuity exists in all of the standard diagrams. From the study of the C abundances, we deduce that the 3rd dredge-up is occurring in all PNe: its efficiency too is higher with lower initial metallicities, offering an easy explanation for the higher number of carbon stars found in metal-deficient galaxies. It is shown that this dredged-up carbon is sometimes transformed into nitrogen by Hot-Bottom Burning, but in a few objects only and not even in all the typeI PNe, which therefore do not form a homogeneous class.
SMC PNe observed and corrected line intensities LMC PNe observed and corrected line intensities Name Planetary nebulae name --- Lambda Wavelength --- Ident Line identification --- Flambda Extinction curve value for Lambda --- l_Fobs Limit flag on Fobs --- Fobs Observed line intensity number=1 scale F(Hbeta)=100 --- u_Fobs Uncertainty flag on Fobs --- l_Fcor Limit flag on Fcor --- Fcor Corrected line intensity number=1 scale F(Hbeta)=100 --- u_Fcor Uncertainty flag on Fcor --- Flux, electronic density and temperature Name Planetary nebula name --- l_Fb Limit flag on Fb --- Fb Flux Hbeta (10-16 erg/cm2/s-1) 10-16mW/m2 e_Fb Hbeta uncertainty % Exp1 IUE exposure number (first number) --- Exp2 IUE exposure number (second number) --- Exp3 IUE exposure number (third number) --- Ne Electronic density cm-3 T(OIII) [OIII] electronic temperature K T(NII) [NII] electronic temperature K Copt Logarithmic extinction constant --- e_Copt rms uncertainty on Copt --- Patricia Bauer CDS 1996 Jan 09 P. Leisy <Leisy@iap.fr> J_A+AS_116_95.xml Stark broadening of solar Mg I lines J/A+AS/117/127 J/A+AS/117/127 Solar MgI lines Stark broadening Stark broadening of solar Mg I lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 117 127 1996 1996A&AS..117..127D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles molecular data Sun: chromosphere Sun: photosphere Using a semiclassical approach, we have calculated electron-, proton-, Mg II-, Si II-, Fe II-, and Ar II- impact line widths and shifts for 267 Mg I multiplets, in order to provide the needed Stark broadening parameters for all important perturbers for investigation of Solar and laboratory plasma. An analysis of Solar Rydberg lines in the far infrared spectrum has been performed as well.
Stark broadening parameters due to e-, p- and Ar II-impacts for Mg I, for perturber density of 1 x 10+11 cm-3 N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K We FWHM for electron impacts (2} 0.1nm de Shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Wp FWHM for proton impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm dp Shift for proton impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm WAr+ FWHM for Ar II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm dAr+ Shift for Ar II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Stark broadening parameters due to Si II-, Fe II- and Mg II-impacts for Mg I, for perturber density of 1 x 10+11 cm-3 N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K WSi+ FWHM for Si II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm dSi+ Shift for Si II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm WFe+ FWHM for Fe II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm dFe+ Shift for Fe II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm WMg+ FWHM for Mg II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm dMg+ Shift for Mg II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Stark broadening parameters due to e-, p- and Ar II-impacts for Mg I, , for perturber densities 1 x 10+15 cm-3 - 1 x 10+19 cm-3 N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for N.V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for N.V > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WAr+ (4) --- WAr+ FWHM for Ar II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dAr+ (4) --- dAr+ shift for Ar II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1996 Jan 18 M.S. Dimitrijevic <mdimitrijevic@aob.aob.bg.ac.yu> J_A+AS_117_127.xml Penetrating the "zone of avoidance". II. Optically detected galaxies in the region 180 <= l <~ 240 J/A+AS/117/1 J/A+AS/117/1 Galaxies in the "zone of avoidance". II. Penetrating the "zone of avoidance". II. Optically detected galaxies in the region 180 <= l <~ 240 R Seeberger W Saurer R Weinberger Astron. Astrophys. Suppl. Ser. 117 1 1996 1996A&AS..117....1S J/A+AS/110/269 : Part I. |b|=5 J/A+AS/117/369 : Part III, 120<l<130, |b|<10 Cross identifications Galaxy catalogs catalogs dust, extinction galaxies: general large-scale structure of universe We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg<=b<=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l>=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.
Optically detected galaxies in the region 180 < l < 210, |b| < 5 Optically detected galaxies in the region 210 < l < 250, |b| < 5 Name Name based on galactic position --- RAh Right ascension B1950 h RAm Right ascension B1950 min RAs Right ascension B1950 s DE- Declination sign --- DEd Declination B1950 deg DEm Declination B1950 arcmin RAh2000 Right ascension J2000 h RAm2000 Right ascension J2000 min RAs2000 Right ascension J2000 s DE-2000 Declination sign --- DEd2000 Declination J2000 deg DEm2000 Declination J2000 arcmin POSS POSS print number --- Xpos Cartesian x-coordinate on POSS mm Ypos Cartesian y-coordinate on POSS mm Diam1 Maximum diameter on POSS-E arcmin Diam1c Maximum diameter of the core on POSS-E arcmin Diam2 Maximum diameter on POSS-O arcmin Diam2c Maximum diameter of the core on POSS-O arcmin u_Diam2c Uncertainty flag on Diam2c --- MType Morphological type --- Rem Cross-identifications and remarks --- Francois Ochsenbein CDS 1995 Dec 20 W. Saurer, <Walter.Saurer@uibk.ac.at> J_A+AS_117_1.xml Determination of effective temperatures for an extended sample of dwarfs and subdwarfs (F0-K5). J/A+AS/117/227 J/A+AS/117/227 Dwarf effective temperatures Determination of effective temperatures for an extended sample of dwarfs and subdwarfs (F0-K5). A Alonso S Arribas C Martinez-Roger Astron. Astrophys. Suppl. Ser. 117 227 1996 1996A&AS..117..227A Effective temperatures Photometry, infrared Stars, subdwarf stars: fundamental parameters stars: general stars: Population II subdwarfs We have applied the InfraRed Flux Method (IRFM) to a sample of 475 dwarfs and subdwarfs in order to derive their effective temperatures with a mean accuracy of about 1.5%. We have used the new homogeneous grid of theoretical model atmosphere flux distributions developed by Kurucz (1991, 1993) for the application of the IRFM. The atmospheric parameters of the stars cover, roughly, the ranges: 3500K<=T_eff_<=8000K; -3.5<=[Fe/H]<=+0.5; 3.5<=log(g)<=5. The monochromatic infrared fluxes at the continuum, and the bolometric fluxes are derived using recent results, which satisfy the accuracy requirements of the work.
Effective temperatures ID Identification number=1 Giclas number has been preferred when available. HD, BD, HR and GJ numbers were used otherwise. The stars are ordered in right ascension --- n_ID Note on ID number=2 1: SB501: Wrong FJ, (J=11.22). 2: G036-050: The error in FJ is greater than 10%, hence no TJ is provided. 3: G178-030: Very faint star, J=11.63, H=11.31 and K=11.127. 4: G167-011: The error in FJ is greater than 20%. The faintest star of the sample (J=12.99). 5: HR6228: Wrong FJ. 6: G017-037: Very faint star, J=11.706, H=11.300 and K=11.297. 7: G021-006: Wrong FJ, (J=10.38). 8: G126-063: Faint star, J=10.69, H=10.64 and K=10.59. 9: G217-008: Wrong FJ. --- logg Surface gravity cm/s2 [Fe/H] Metallicity --- FBol Bolometric flux 10-2mW/m2 E(B-V) Interestellar redenning mag FJ Monochromatic flux in the band J 10-2mW/m2 qJ q-factor in the band J --- l_TJ limit flag on TJ --- TJ Temperature derived in the band J K n_TJ )] Note on TJ number=3 A bracket indicates that the temperature has not been considered in the mean as explained in Sect. 5. A parentheses indicates temperatures under 4000 K. In this case there isn't estimation of the total error because of the uncertainties of the model fluxes in this range. --- e_TJ rms uncertainty on TJ number=4 Error computed considering errors in FBol, FJ, logg and [Fe/H]. K FH Monochromatic flux in the band H 10-2mW/m2 qH q-factor in the band H --- l_TH Limit flag on TH --- TH Temperature derived in the band H K n_TH []] Note on TH number=3 A bracket indicates that the temperature has not been considered in the mean as explained in Sect. 5. A parentheses indicates temperatures under 4000 K. In this case there isn't estimation of the total error because of the uncertainties of the model fluxes in this range. --- e_TH rms uncertainty on TH number=4 Error computed considering errors in FBol, FJ, logg and [Fe/H]. K FK Monochromatic flux in the band K 10-2mW/m2 qK q-factor in the band K --- TK Temperature derived in the band K K e_TK rms uncertainty on TK number=4 Error computed considering errors in FBol, FJ, logg and [Fe/H]. K Tmean Weighted mean temperature derived from TJ, TH and TK K n_Tmean Note on Tmean number=3 A bracket indicates that the temperature has not been considered in the mean as explained in Sect. 5. A parentheses indicates temperatures under 4000 K. In this case there isn't estimation of the total error because of the uncertainties of the model fluxes in this range. --- e_Tmean rms uncertainty on Tmean number=5 Mean error computed considering linear transmission of errors from e_TJ, e_TH and e_TK. K table4a.tex LaTeX version of table4, part 1 table4b.tex LaTeX version of table4, part 2 Patricia Bauer CDS 1996 Jan 18 Angel Alonso <aas@ll.iac.es> J_A+AS_117_227.xml Surface photometry of galaxies in low density regions. J/A+AS/117/261 J/A+AS/117/261 BR photometry of galaxies in low density regions Surface photometry of galaxies in low density regions. J Vennik U Hopp B Kovachev B Kuhn H Elsaesser Astron. Astrophys. Suppl. Ser. 117 261 1996 1996A&AS..117..261V Photometry, surface galaxies: fundamental parameters galaxies: photometry galaxies: structure large-scale structure of universe We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_<-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_>=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.
Observed model-free photometric data in B and colour characteristics Observed model-free photometric data in R Name Galaxy designation according to Hopp et al. (1995) or UGC (Nilson, 1973) or CGCG (Zwicky et al., 1961-68) --- RAh Right ascension (1950) hours h RAm Right ascension (1950) minutes min RAs Right ascension (1950) seconds s DE- Declination sign --- DEd Declination (1950) degrees deg DEm Declination (1950) arcminutes arcmin DEs Declination (1950) arcseconds arcsec Colour Colour considered, B or R --- MTmag Asymptotic B or R magnitude number=1 M stands for B or R, B in table5, R in table6 mag M25mag Integrated magnitude within 25-th B or R magnitude isophote number=1 M stands for B or R, B in table5, R in table6 mag rad25 Equivalent radius at the 25-th B or R magnitude isophote mag b/a Minor-to-major axis ratio --- PA Position angle deg u_PA Uncertainty flag on PA --- muM,0 Central surface brightness number=1 M stands for B or R, B in table5, R in table6 mag/arcsec+2 u_muM,0 Uncertainty flag on muM,0 number=1 M stands for B or R, B in table5, R in table6 --- radeff Effective (equivalent) radius arcsec (B-R)0 Central (B-R) colour index mag (B-R)T Integral (B-R) colour index mag u_(B-R)T Uncertainty flag on (B-R)T --- D(B-R)/Dr Radial colour gradient mag/arcsec e_D(B-R)/Dr 1 sigma error of the colour gradient mag/arcsec Reduced photometric data and exponential model parameters in B Reduced photometric data and exponential model parameters in R Name Galaxy designation according to Hopp et al.(1995) or UGC (Nilson, 1973) or CGCG (Zwicky et al., 1961-68) --- Dist Distance Mpc Colour Colour considered, B or R --- Mag Absolute magnitude mag radEff Effective (equivalent) radius kpc u_radEff Uncertainty flag on radeff --- muEff Effective surface brightness mag/arcsec+2 1/alpha1 Exponential scale length arcsec u_1/alpha1 Uncertainty flag on 1/alpha1 --- 1/alpha2 Exponential scale length kpc u_1/alpha2 Uncertainty flag on 1/alpha2 --- mu0 Exponential model central surface brightness mag/arcsec+2 u_mu0 Uncertainty flag on mu0 --- mu0,c Corrected central surface brightness mag/arcsec+2 u_mu0,c Uncertainty flag on mu0,c --- n Parameter n of the best fitting power law --- u_n Uncertainty flag on n --- Type Profile type --- Class Isolation class --- Patricia Bauer CDS 1996 Mar 26 J_A+AS_117_261.xml uvby-{beta} photometry of high-velocity and metal-poor stars. VIII. Stars of very low metal abundance. J/A+AS/117/317 J/A+AS/117/317 uvby-beta photometry of metal-poor stars. VIII. uvby-{beta} photometry of high-velocity and metal-poor stars. VIII. Stars of very low metal abundance. W J Schuster P E Nissen L Parrao T C Beers L P Overgaard Astron. Astrophys. Suppl. Ser. 117 317 1996 1996A&AS..117..317S II/180 : uvby-beta photometry of metal-poor stars. III. (Schuster+ 1989) J/A+AS/97/951 : uvby-beta photometry of metal-poor stars. VI. (Schuster+ 1993) Schuster at al., Paper I. 1988A&AS...73..225S Schuster at al., Paper II. 1989A&A...221...65S Schuster at al., Paper III. 1989A&A...222...69S, Cat. <II/180> Allen et al., Paper IV. 1991A&A...244..280A Nissen et al., Paper V. 1991A&A...251..457N Schuster et al. Paper VI. 1993A&AS...97..951S, Cat. <J/A+AS/97/951> Marquez et al., Paper VII. 1994A&AS..108..341M Schuster at al., Paper IX. 1997A&A...319..796S Abundances, [Fe/H] Photometry, uvby, beta Stars, high-velocity Stars, metal-deficient dust, extinction Galaxy: evolution Galaxy: halo stars: abundances stars: distances stars: fundamental parameters A catalogue of uvby-{beta} photometry for 87 of the turn-off and subgiant stars from the HK survey of Beers et al. (1992AJ....103.1987B, BPSII) is given. Most of these stars have [Fe/H]<=2.5. These photometric data have been taken and reduced using the same techniques as in our previous two uvby-{beta} catalogues (Schuster et a., 1989, Cat. <II/180> and Schuster et al., 1993, Cat. <J/A+AS/97/951>). An error analysis has been made; typical mean observational errors for a star with V=14.2m are 0.008, 0.007, 0.011, 0.010 and 0.012 in V, (b-y), m_1_, c_1_ and {beta}, respectively. Our photometric data are also compared to the UBV photometry and spectral indices from the HK survey; satisfactory agreement is found indicating good quality for the two data sets. The stars are classified in reddening-free diagrams of the uvby-{beta} system; several of the stars are found to have been mis-classified in the HK survey. Two metal-poor supergiants, three (possibly four) horizontal branch stars, one blue subluminous star and two stars with ambiguous photometry have been identified. Stellar parameters, such as E(b-y), M_V_, {delta}M_V_, and T_eff_, plus error estimates for these parameters, are provided using our photometric calibrations. Although all stars have galactic latitudes |b|>=30{deg} many of them are significantly reddened with E(b-y) ranging from 0.02 to 0.15. The average reddening towards the South Galactic Pole region, b<-60{deg}, is E(b-y)=0.027+/-0.004 corresponding to E(B-V)=0.036+/-0.005 in contrast to the low value of E(B-V)~0.01 derived from the Burstein & Heiles (1982AJ.....87.1165B) maps. The stars are analyzed in the (b-y)_0_, [Fe/H] diagram, and individual ages estimated using the isochrones of VandenBerg & Bell (1985ApJS...58..561V) and of Bergbusch & VandenBerg (1992ApJS...81..163B). These very metal-poor stars are found to be coeval, within 1-2Gyr, with the halo and thick-disk stars studied previously, with a mean age in excess of 18Gyr. Several blue "thick-disk" stars, which are perhaps analogous to the "blue metal-poor" stars of Preston et al. (1994, Cat. <J/AJ/108/538>), have been identified.
The standard uvby-{beta} catalogue for the 87 BPSII (Beers et al., 1992AJ....103.1987B) stars Star Star designation according to BPSII (Beers et al., 1992AJ....103.1987B) --- Vmag V magnitude mag b-y b-y colour index mag m1 m1 colour index mag c1 c1 colour index mag o_b-y Number of independent uvby observations --- beta beta colour index mag o_beta Number of independent beta observations --- Note Note --- Stellar parameters for the 86 VMP stars. Star Star designation according to BPSII (Beers et al., 1992AJ....103.1987B) --- E(b-y) Reddening mag e_E(b-y) rms uncertainty on E(b-y) mag [Fe/H]c Spectroscopic metallicity [Sun] [Fe/H]p Photometric metallicity [Sun] u_[Fe/H]p Uncertainty flag on [Fe/H]p --- e_[Fe/H]p rms uncertainty on [Fe/H]p [Sun] MV Absolute V magnitude mag e_MV rms uncertainty on MV mag dMV Evolutionnary correction {delta}MV (See Nissen et al., 1991A&A...251..457N) mag e_dMV rms uncertainty on dMV mag Teff Effective temperature K e_Teff rms uncertainty on Teff K James Marcout, Patricia Bauer CDS 1997 Sep 12 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_117_317.xml Optical positions of radio emitting stars. J/A+AS/117/335 J/A+AS/117/335 Optical positions of radio emitting stars Optical positions of radio emitting stars. M Assafin A H Andrei S P Puliaev E G Jilinski R Vieira Martins G G Vieira W M de Oliveira Astron. Astrophys. Suppl. Ser. 117 335 1996 1996A&AS..117..335A Positional data Stars, radio astrometry radio continuum: stars reference systems In order to contribute to the alignment of the radio and optical reference frames, 50 stars with confirmed radio emission and published radio positions were observed by astrographical means. Additionally, two confirmed radio-stars of fainter magnitude were observed using a CCD direct camera with a long focus, large aperture telescope. The reductions are made relative to four catalogues: the Carlsberg Meridian Catalogue #4, the International Reference Stars Catalogue, the Positions and Proper Motion Catalogue and the Astrographical Catalogue of Reference Stars. The best results were obtained with the CAMC catalogue. The plate error of a radio star position is 0.07" for both right ascension and declination, rising to 0.10"-0.20" for bright stars. Ten of the program stars are not in the HIPPARCOS Input Catalogue and 12 do not belong to any of the major reference catalogues used. As soon as the HIPPARCOS results become available, its reference stars already measured in the plates will enable us to get positions for those 10 radio stars in the HIPPARCOS system.
Positions obtained astrographically and their comparison against major optical catalogues Positions obtained by mosaicing of CCD images and their comparison against major optical catalogues Name Name of the radio star --- Vmag Visual magnitude mag Sp Spectral type --- Ep-1900 Epoch of the astrographic observation (1900+) yr RAh Right ascension (J2000), at epoch number=1 RA and DE are referred to CAMC#4 catalogue h RAm Right ascension (J2000), at epoch number=1 RA and DE are referred to CAMC#4 catalogue min RAs Right ascension (J2000), at epoch number=1 RA and DE are referred to CAMC#4 catalogue s e_RAs rms uncertainty on right ascension s DE- Declination sign --- DEd Declination (J2000), at epoch number=1 RA and DE are referred to CAMC#4 catalogue deg DEm Declination (J2000), at epoch number=1 RA and DE are referred to CAMC#4 catalogue arcmin DEs Declination (J2000), at epoch number=1 RA and DE are referred to CAMC#4 catalogue arcsec e_DEs rms uncertainty on declination arcsec DRA Difference in RA with CAMC#4 arcsec DDE Difference in DE with CAMC#4 arcsec DRA2 Difference in RA with ACRS arcsec DDE2 Difference in DE with ACRS arcsec DRA3 Difference in RA with PPM arcsec DDE3 Difference in DE with PPM arcsec DRA4 Differences in RA with the PPM High Precision Subset arcsec DDE4 Difference in DE with the PPM High Precision Subset arcsec DRA5 Difference in RA with IRS arcsec DDE5 Difference in DE with IRS arcsec Patricia Bauer CDS 1996 Mar 26 M. Assafin, <massaf@dans.on.br> J_A+AS_117_335.xml Penetrating the 'zone of avoidance': III. A survey for obscured galaxies in the region 120<l<130,-10<b<+10 J/A+AS/117/369 J/A+AS/117/369 Galaxies in the "zone of avoidance". III. Penetrating the 'zone of avoidance': III. A survey for obscured galaxies in the region 120<l<130,-10<b<+10 G Lercher F Kerber R Weinberger Astron. Astrophys. Suppl. Ser. 117 369 1996 1996A&AS..117..369L J/A+AS/110/269 : Part I., |b|=5 J/A+AS/117/1 : Part II, 180<l<240 Cross identifications Galaxy catalogs catalogs dust, extinction galaxies: clusters: general galaxies: general Galaxy: structure As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg<=l<=130deg, -10deg<=b<=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.
optically detected galaxies in the region 120<l<130, -10<b<+10 Name Object designation based on galactic position --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec RAh2000 Right ascension (2000.0) h RAm2000 Right ascension (2000.0) min RAs2000 Right ascension (2000.0) s DEd2000 Declination (2000.0) deg DEm2000 Declination (2000.0) arcmin DEs2000 Declination (2000.0) arcsec POSS POSS-I print label --- Xpos Cartesian x-coordinate on POSS mm Ypos Cartesian y-coordinate on POSS mm DmajE Maximum diameter on POSS-E arcmin DminE Minimum diameter on POSS-E arcmin DmajEc Maximum diameter of core on POSS-E arcmin DminEc Minimum diameter of core on POSS-E arcmin DmajO Maximum diameter on POSS-O arcmin DminO Minimum diameter on POSS-O arcmin DmajOc Maximum diameter of core on POSS-O arcmin DminOc Minimum diameter of core on POSS-O arcmin MType Morphological type --- Ident Cross identifications --- Patricia Bauer CDS 1996 Feb 01 G. Lercher <Georg.Lercher@uibk.ac.at> J_A+AS_117_369.xml Far infrared properties of Hickson compact groups of galaxies. I. High resolution IRAS maps and fluxes J/A+AS/117/39 J/A+AS/117/39 Hickson Compact Groups of Galaxies I. Far infrared properties of Hickson compact groups of galaxies. I. High resolution IRAS maps and fluxes S Allam R Assendorp G Longo M Braun G Richter Astron. Astrophys. Suppl. Ser. 117 39 1996 1996A&AS..117...39A VII/85 : Catalogue of compact groups of galaxies (Hickson, 1982) II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) J/ApJ/380/30 : LF of Compact Groups (Mendes de Oliveira+ 1991) J/ApJ/399/353 : Radial velocities in Hickson Compact Groups (Hickson+ 1992) Hickson P., 1982, ApJ, 255, 382 =Catalogue <VII/85> Hickson P., 1993, Atlas of Compact Groups of Galaxies, Astrophys. Lett. & Commun., 29, 1 =1993ApL....29....1H Clusters, galaxy Galaxies, IR atlases galaxies: clusters: general infrared: galaxies The Far Infrared (FIR) properties of galaxies which are members of compact groups bear relevant information on the dynamical status and the physical properties of these structures. All studies published so far have been undermined by the poor sensitivity and spatial resolution of the IRAS-PSC and IRAS Sky Survey data. We used the HIRAS software available at the IRAS server at the Laboratory for Space Research in Groningen to fully exploit the redundancy of the IRAS data and to approach the theoretical diffraction limit of IRAS. Among the 97 groups which were observed by IRAS, 62 were detected in at least one band, while reliable upper limits were derived for all the others. Among the detected groups, 49 were fully or partially resolved, i.e. it was possible to discriminate which member or members emit most of the FIR light. At 60{mu}m, for instance, 87 individual sources were detected in 62 groups. In order to ease the comparison with data obtained at other wavelengths - and in particular in the X and radio domains - we give co-added and HIRAS maps for all the detected groups.
Flux and upper limits for galaxies which are members of the Hickson's Groups. HCG Identification accordingly to Hickson (1982) number=1 If the group is not detected in any of the IRAS bands there is only one entry --- Mtype Morphological type of the galaxy accordingly to Hickson (1993) --- l_F12 Upper limit on F12 --- F12 Flux at 12{mu}m Jy n_F12 Note on F12 number=2 When the FIR source corresponds to several unresolved members of the group, we give (in brackets) the list of the members which fall within the FIR source --- e_F12 rms uncertainty on F12 mJy l_F25 Upper limit on F25 --- F25 Flux at 25{mu}m Jy n_F25 Note on F25 number=2 When the FIR source corresponds to several unresolved members of the group, we give (in brackets) the list of the members which fall within the FIR source --- e_F25 rms uncertainty on F25 mJy l_F60 Upper limit on F60 --- F60 Flux at 60{mu}m Jy n_F60 Note on F60 number=2 When the FIR source corresponds to several unresolved members of the group, we give (in brackets) the list of the members which fall within the FIR source --- e_F60 rms uncertainty on F60 mJy l_F100 Upper limit on F100 --- F100 Flux at 100{mu}m Jy n_F100 Note on F100 number=2 When the FIR source corresponds to several unresolved members of the group, we give (in brackets) the list of the members which fall within the FIR source --- e_F100 rms uncertainty on F100 mJy Com Comments --- table2.tex LaTeX version of table2 Patricia Bauer CDS 1996 Mar 15 J_A+AS_117_39.xml Near-infrared surface photometry of spiral galaxies. I. The data. J/A+AS/117/417 J/A+AS/117/417 Inclined Sa-Scd galaxies surface photometry Near-infrared surface photometry of spiral galaxies. I. The data. P Heraudeau F Simien G A Mamon Astron. Astrophys. Suppl. Ser. 117 417 1996 1996A&AS..117..417H Photometry, infrared Photometry, surface Photometry, UBVRI galaxies: photometry galaxies: spiral infrared: galaxies We present K'-band surface photometry of a sample of 31 inclined Sa-Scd galaxies, together with additional J- and H-band data for four of them. In this first paper of a series, profiles are presented, together with global and isophotal parameters. Our profiles are compared to similar B, R and I data collected from other sources. Three galaxies exhibit previously unknown small bars in their center while in five others, such bars may also be present. Four objects present a narrow elongated feature in their center aligned with their major axis, which could be an inward extension of the disk. A few galaxies display very thin spiral arms. Color-color diagrams indicate that the extinction inside the four galaxies for which we have JHK' images is limited to A_V<2.
Catalog parameters and exposure times No Sequence number --- Name1 Object identification: ESO number, if any --- Name2 Other identification, if any: NGC, IC, MCG --- MType Morphological type --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Bt Integrated B magnitude mag D25 Apparent diameter at brightness mu_B=25 arcmin cz Heliocentric radial velocity km/s Dist Distance number=1 Distance determined (with H0=75 km/s/Mpc), from cz corrected for Virgocentric infall. Mpc Exp Total exposure time in K' s Photometric profiles in J, H, K' and/or B, R, for four galaxies Name Object identification (ESO or NGC number) --- Rad Semi-major axis arcsec PA Position angle (in K') deg eps ellipticity (in K') --- muB Surface brightness per square arcsec, in B mag muR Surface brightness per square arcsec, in R mag muJ Surface brightness / sq. arcsec, in J mag e_muJ one-sigma rms error on mu_J mag muH Surface brightness / sq. arcsec, in H mag e_muH one-sigma rms error on mu_H mag muK' Surface brightness / sq. arcsec, in K' mag e_muK' one-sigma rms error on mu_K' mag Photometric profiles in K' and/or B, V, R, I, for 27 galaxies Name Object identification (ESO or NGC number) --- Rad Semi-major axis arcsec PA Position angle (in K') deg eps ellipticity (in K') --- muB Surface brightness / sq. arcsec, in B mag muV Surface brightness / sq. arcsec, in V mag muR Surface brightness / sq. arcsec, in R mag muI Surface brightness / sq. arcsec, in I mag muK' Surface brightness / sq. arcsec, in K' mag e_muK' one-sigma rms error on mu_K' mag Isophote-shape parameters for 13 galaxies Name Object identification (ESO, IC, or NGC number) --- mu_K' K'-band surface brightness of isophote mag Rad Semi-major axis of best-fitting ellipse number=1 Due to a different fitting algorithm, these parameters can be slightly different than those given in Table 2a, for the same isophote; for innermost isophotes, preference is given to the values given in the present Table. arcsec PA Position angle of best-fitting ellipse number=1 Due to a different fitting algorithm, these parameters can be slightly different than those given in Table 2a, for the same isophote; for innermost isophotes, preference is given to the values given in the present Table. deg q Axial ratio of best-fitting ellipse number=1 Due to a different fitting algorithm, these parameters can be slightly different than those given in Table 2a, for the same isophote; for innermost isophotes, preference is given to the values given in the present Table. --- e4 Fourier shape coefficient --- e6 Fourier shape coefficient --- e8 Fourier shape coefficient --- Results of the photometric analysis No Sequence number --- Name1 Object identification: ESO number, if any --- Name2 Other identification, if any: NGC, IC, MCG --- PA Position angle of major axis (N through E) deg Eps Outer ellipticity (at mu_K'=19.5) --- Jt Total magnitude in the J band mag Ht Total magnitude in the H band mag Kt Total magnitude in the K band mag D25_B Apparent diameter at muB=25 number=1 Recomputed from ESO-LV images with a corrected sky brightness, when relevant. arcmin D20_J Apparent diameter at muJ=20 arcmin D19_H Apparent diameter at muH=19 arcmin D19_K Apparent diameter at muK=19 arcmin D20_K Apparent diameter at muK=20 arcmin Heraudeau ? 1996 Mar 11 P. Heraudeau, <heraudeau@obs.univ-lyon1.fr> J_A+AS_117_417.xml An image database. II. Catalogue between {delta}=-30deg and {delta}=70deg. J/A+AS/117/467 J/A+AS/117/467 Image of Galaxies data-base II. An image database. II. Catalogue between {delta}=-30deg and {delta}=70deg. R Garnier G Paturel C Petit M C Marthinet J Rousseau Astron. Astrophys. Suppl. Ser. 117 467 1996 1996A&AS..117..467G VII/155 : Third Reference Catalog of Bright Galaxies (de Vaucouleurs+ 1991) VII/119 : Catalogue of Principal Galaxies (PGC) (Paturel+ 1989) http://www-obs.univ-lyon1.fr/leda/ : The LEDA databasede Vaucouleurs G., de Vaucouleurs A., Corwin H.G. Jr, Buta R.J., Paturel G., Fouque P., 1991, Third Reference Catalog of Bright Galaxies, Springer-Verlag (RC3), Cat. <VII/155> Garnier R., Paturel G., Petit C., Marthinet M.C., Rousseau J., 1996A&AS..117..467G Paturel G., Fouque P., Bottinelli L., Gouguenheim L., 1989A&AS...80..299P, Cat. <VII/119> Paturel G., Fouque P., Bottinelli L., Gouguenheim L., 1989b, Catalog of Principal Galaxies, Monographies de la Base de Donnees Extragalactiques No1, vol. 1,2,3, Observatoire de Lyon (updated version in 1996 on CD-ROM) Paturel G., Garnier R., Petit C., Marthinet M.C., 1996A&A...311...12P Galaxy catalogs catalogs galaxies: general galaxies: photometry A preliminary list of 68.040 galaxies was built from extraction of 35.841 digitized images of the Palomar Sky Survey (Paper I, 1996A&A...311...12P). For each galaxy, the basic parameters are obtained: coordinates, diameter, axis ratio, total magnitude, position angle. On this preliminary list, we apply severe selection rules to get a catalog of 28.000 galaxies, well identified and well documented. For each parameter, a comparison is made with standard measurements. The accuracy of the raw photometric parameters is quite good despite of the simplicity of the method. Without any local correction, the standard error on the total magnitude is about 0.5 magnitude up to a total magnitude of B_T_=17. Significant secondary effects are detected concerning the magnitudes: distance to plate center effect and air-mass effect. The description of the construction of the catalog is given in Paturel et al. 1996 and Garnier et al. 1996. Galaxies are detected on POS-I and cross-identified with galaxies from the LEDA database (http://www-obs.univ-lyon1.fr/leda/)
The Catalogue PGC Name according to Paturel et al. (1989, Cat. <VII/119>) --- Name Alternate name in a hierarchy number=1 NGC, IC, UGC, ESO, MCG, CGCG (see Paturel et al. 1989, Cat. <VII/119>) --- RAh Right ascension for 1950 h RAm Right ascension for 1950 min RAs Right ascension for 1950 s DE- Declination sign --- DEd Declination for 1950 deg DEm Declination for 1950 arcmin DEs Declination for 1950 arcsec n_Pos *: Accurate coordinates better than 10" --- PA Position angle from North Eastwards deg e_PA rms uncertainty on PA deg BT Total B-magnitude in the RC3 system (de Vaucouleurs et al. 1991, Cat. <VII/155>) mag e_BT rms uncertainty on BT mag logD25 Decimal log of apparent diameter in the RC3 system (up to the isophote 25mag/arcsec^2^) 0.1arcmin e_logD25 rms uncertainty on logD25 0.1arcmin logR25 Decimal log of axis ratio (major axis/ minor axis) in the RC3 system --- e_logR25 rms uncertainty on logR25 --- Patricia Bauer CDS 1997 Mar 24 We thank G. Paturel <paturel@obs.univ-lyon1.fr> for providing a copy of the catalog. J_A+AS_117_467.xml Automatic optical monitoring of 10 blazars. J/A+AS/117/475 J/A+AS/117/475 BVRcIc photometry of 10 blazars Automatic optical monitoring of 10 blazars. M Fiorucci G Tsoti Astron. Astrophys. Suppl. Ser. 117 475 1996 1996A&AS..117..475F BL Lac objects Photometry, UBV BL Lacertae objects: general galaxies: active We report the BVR_c_I_c_ data for 10 blazars observed in the first phase of a long-term photometric monitoring program of about 30 objects. The observations were carried out with a 0.40-m automatic imaging telescope, recently developed by our group at the Perugia University Observatory. During our period of observation 1215+303 and 1424+240 were at their highest values of magnitude, while 0754+100 and 0829+043 displayed large amplitude flares. We further report optical data of Mrk 501 during the same period in which TeV {gamma}-rays were detected by the Whipple Observatory. For a description of the (RI)c photometric system, see e.g. the General Catalog of Photometry Data <GCPD/54>.
List of BVRcIc data Name Blazar name --- Date UT date --- HJD Heliocentric Julian date d l_Bmag Limit flag on B magnitude --- Bmag B magnitude mag e_Bmag rms uncertainty on B magnitude mag Vmag V magnitude mag e_Vmag rms uncertainty on V magnitude mag Rcmag Cousins Rc magnitude mag e_Rcmag rms uncertainty on Rc magnitude mag Icmag Cousins Ic magnitude mag e_Icmag rms uncertainty on Ic magnitude mag Patricia Bauer CDS 1996 Mar 26 J_A+AS_117_475.xml Einstein A-coefficients for vib-rotational transitions in CO J/A+AS/117/557 J/A+AS/117/557 Einstein coefficients for CO transitions Einstein A-coefficients for vib-rotational transitions in CO S Chandra V U Maheshwari A K Sharma Astron. Astrophys. Suppl. Ser. 117 557 1996 1996A&AS..117..557C J/A+AS/114/175 : Einstein A-coefficient for vibrational transitions in CS Atomic physics ISM: molecules molecular data Einstein A-coefficients for vib-rotational transitions in CO isotopomers, for vibrational quantum number v up to 20, rotational quantum number J up to 140, and {DELTA}v up to 4, are calculated. The change in J is governed by the selection rules {DELTA}J=+/-1. These coefficients play an important role in astronomy, as CO is the most abundant molecule after H_2_, and has been observed in almost all the astronomical objects.
Einstein A-coefficient, energy of lower level, and frequency of transition for C^12^O^16^ Einstein A-coefficient, energy of lower level, and frequency of transition for C^12^O^17^ Einstein A-coefficient, energy of lower level, and frequency of transition for C^12^O^18^ Einstein A-coefficient, energy of lower level, and frequency of transition for C^13^O^16^ Vlow Vibrational quantum number of the lower level --- Jlow Rotational quantum number of the lower level --- Vup Vibrational quantum number of the upper level --- Jup Rotational quantum number of the upper level --- A Einstein A-coefficient s-1 Elow Energy of the lower level of the transition cm-1 Freq Frequency of the transition cm-1 Patricia Bauer CDS 1995 Dec 08 Suresh Chandra <sch@iucaa.iucaa.ernet.in> J_A+AS_117_557.xml Analytic representations of rovibrational dipole matrix elements for the CO molecule and its isotopomers. J/A+AS/117/561 J/A+AS/117/561 Rovibrational dipole matrix elements for CO Analytic representations of rovibrational dipole matrix elements for the CO molecule and its isotopomers. J M Hure E Roueff Astron. Astrophys. Suppl. Ser. 117 561 1996 1996A&AS..117..561H Atomic physics ISM: molecules molecular data Expansion coefficients of the polynomial expansion representing the transition D-values for the {DELTA}v=1 band and the ^12^C^16^O isotope. Results are obtained using the Electric Dipole Moment Function EDMF2 (Langhoff & Bauschlicher 1995, J. Chem. Phys. 102, 5220). The fits are better than 1% when |m|<=m_max_.
DELTAv=1 for 12C16O DELTAv=2 for 12C16O DELTAv=3 for 12C16O DELTAv=1 for 13C16O DELTAv=2 for 13C16O DELTAv=3 for 13C16O DELTAv=1 for 12C17O DELTAv=2 for 12C17O DELTAv=3 for 12C17O DELTAv=1 for 12C18O DELTAv=2 for 12C18O DELTAv=3 for 12C18O v'' Lower vibrational quantum number --- [m_max_] Rotationless transition matrix element D a0 Constant for n=DELTAv number=1 Each sequence and each vibrational band have been fitted with a fourth order polynomial form by using a numerical minimax procedure from the Nag mathematical library as a function of m=[J'(J'+1)-J"(J"+1)]/2, v" and {DELTA}v=n D^v"^_n_(m)=<v"+n, J"|M|v", J"> =a0(v",n)+a1(v",n)m+a2(v",n)m^2^+a3(v",n)m^3^+a4(v",n)m^4^ --- a1 First-order coefficient for n=DELTAv number=1 Each sequence and each vibrational band have been fitted with a fourth order polynomial form by using a numerical minimax procedure from the Nag mathematical library as a function of m=[J'(J'+1)-J"(J"+1)]/2, v" and {DELTA}v=n D^v"^_n_(m)=<v"+n, J"|M|v", J"> =a0(v",n)+a1(v",n)m+a2(v",n)m^2^+a3(v",n)m^3^+a4(v",n)m^4^ --- a2 Second-order coefficient for n=DELTAv number=1 Each sequence and each vibrational band have been fitted with a fourth order polynomial form by using a numerical minimax procedure from the Nag mathematical library as a function of m=[J'(J'+1)-J"(J"+1)]/2, v" and {DELTA}v=n D^v"^_n_(m)=<v"+n, J"|M|v", J"> =a0(v",n)+a1(v",n)m+a2(v",n)m^2^+a3(v",n)m^3^+a4(v",n)m^4^ --- a3 Thrid-order coefficient for n=DELTAv number=1 Each sequence and each vibrational band have been fitted with a fourth order polynomial form by using a numerical minimax procedure from the Nag mathematical library as a function of m=[J'(J'+1)-J"(J"+1)]/2, v" and {DELTA}v=n D^v"^_n_(m)=<v"+n, J"|M|v", J"> =a0(v",n)+a1(v",n)m+a2(v",n)m^2^+a3(v",n)m^3^+a4(v",n)m^4^ --- a4 Fourth-order coefficient for n=DELTAv number=1 Each sequence and each vibrational band have been fitted with a fourth order polynomial form by using a numerical minimax procedure from the Nag mathematical library as a function of m=[J'(J'+1)-J"(J"+1)]/2, v" and {DELTA}v=n D^v"^_n_(m)=<v"+n, J"|M|v", J"> =a0(v",n)+a1(v",n)m+a2(v",n)m^2^+a3(v",n)m^3^+a4(v",n)m^4^ --- Patricia Bauer CDS 1996 Apr 25 J_A+AS_117_561.xml Spectra of late type stars from 4800 to 9000 Angstroems J/A+AS/117/93 J/A+AS/117/93 Spectra of 21 late-type stars Spectra of late type stars from 4800 to 9000 Angstroems M Serote Roos C Boisson M Joly Astron. Astrophys. Suppl. Ser. 117 93 1996 1996A&AS..117...93S J/A+AS/116/239 : Spectra in H band (Dallier+, 1996) Spectroscopy atlases stars: abundances stars: fundamental parameters stars: late-type supergiants We present optical spectra of 21 stars from 4800 to 8920A, covering essentially the late spectral types, G, K, M and the luminosity classes I and III. Half of the stars are super metal rich (SMR) ones. The spectra were obtained at a resolution of 1.25A using the Aurelie spectrograph, equipped with a linear array CCD-like detector, attached to the OHP 1.52m telescope. Also presented are the spectra of 7 stars, covering the region 5000-9783A at a resolution of 8.5A, observed at the CFHT with the Herzberg spectrograph. The spectral types are F, G, K, M and the luminosity classes III and V. Five stars are SMR. These spectra have been obtained with the aim of extending existing libraries used for population synthesis purposes. The inclusion of SMR stars in a stellar library dedicated to the study of stellar populations in the central part of galaxies is crucial as abundance gradients have been observed in the optical range.
HD 36395 Gliese 205 (CFH) M1VSMR 05 31 24.8 -03 38 54 HD 38858 HR 2007 (CFH) G4V 05 48 34.7 -04 05 29 HD 39715 Gliese 223 (CFH) K3VSMR 05 54 28.1 +02 09 06 HD 72184 HR 3360 (CFH) K2IIISMR 08 32 55.4 +38 01 07 HD 72324 32 Cnc (CFH) G9IIISMR 08 33 00.3 +24 05 07 HD 88815 HR 4016 (CFH) F2V 10 18 01.7 +73 04 28 HD 93800 (CFH) K0VSMR 10 49 32.3 -06 46 13 HD 112127 (OHP) K2IIISMR 12 53 55.6 +26 46 48 HD 120315 85 UMa (OHP) B3V 13 47 33.0 +49 18 48 HD 121370 eta Boo (OHP) G0IVSMR 13 54 41.2 +18 24 10 HD 123657 BY Boo (OHP) M5III 14 07 55.6 +43 51 17 HD 139669 theta UMi (OHP) K5IIISMR 15 31 25.5 +77 20 57 HD 139195 16 Ser (OHP) K0IIImp 15 36 29.4 +10 00 43 HD 141477 kappa Ser (OHP) M0III 15 48 44.5 +18 08 34 HD 145675 14 Her (OHP) K0VSMR 16 10 23.6 +43 49 18 HD 148856 beta her (OHP) G7IIIa 16 30 13.5 +21 29 23 HD 156283 pi Her (OHP) K3IISMR 17 15 02.9 +36 48 33 HD 159181 beta Dra (OHP) G2IabSMR 17 30 26.0 +52 18 04 HD 160762 iota Her (OHP) B3IV 17 39 27.8 +46 00 23 HD 161797 mu Her (OHP) G5IVSMR 17 46 28.6 +27 43 52 HD 163993 xi Her (OHP) G8IIISMR 17 57 45.5 +29 14 53 HD 168532 105 Her (OHP) K4IImp 18 19 10.6 +24 26 45 HD 176670 lambda Lyr (OHP) K3IIISMR 19 00 00.7 +32 08 43 HD 181984 tau Dra (OHP) K3IIISMR 19 15 34.5 +73 21 14 HD 180809 theta Lyr (OHP) K0IImp 19 16 22.0 +38 08 01 HD 185622 HR 7475 (OHP) M0Iab 19 39 25.3 +16 34 17 HD 196725 theta Del (OHP) K3IbSMR 20 38 43.9 +13 18 54 HD 206936 mu Cep (OHP) M2Ia 21 43 30.3 +58 46 48
hd36395.fit Spectrum of HD 36395 (M1VSMR) hd38858.fit Spectrum of HD 38858 (G4V) hd39715.fit Spectrum of HD 39715 (K3VSMR) hd72184.fit Spectrum of HD 72184 (K2IIISMR) hd72324.fit Spectrum of HD 72324 (G9IIISMR) hd88815.fit Spectrum of HD 88815 (F2V) hd93800.fit Spectrum of HD 93800 (K0VSMR) hd112127.fit Spectrum of HD 112127 (K2IIISMR) hd120315.fit Spectrum of HD 120315 (B3V) hd121370.fit Spectrum of HD 121370 (G0IVSMR) hd123657.fit Spectrum of HD 123657 (M5III) hd139195.fit Spectrum of HD 139195 (K0IIImp) hd139669.fit Spectrum of HD 139669 (K5IIISMR) hd141477.fit Spectrum of HD 141477 (M0III) hd145675.fit Spectrum of HD 145675 (K0VSMR) hd148856.fit Spectrum of HD 148856 (G7IIIa) hd156283.fit Spectrum of HD 156283 (K3IISMR) hd159181.fit Spectrum of HD 159181 (G2IabSMR) hd160762.fit Spectrum of HD 160762 (B3IV) hd161797.fit Spectrum of HD 161797 (G5IVSMR) hd163993.fit Spectrum of HD 163993 (G8IIISMR) hd168532.fit Spectrum of HD 168532 (K4IImp) hd176670.fit Spectrum of HD 176670 (K3IIISMR) hd180809.fit Spectrum of HD 180809 (K0IImp) hd181984.fit Spectrum of HD 181984 (K3IIISMR) hd185622.fit Spectrum of HD 185622 (M0Iab) hd196725.fit Spectrum of HD 196725 (K3IbSMR) hd206936.fit Spectrum of HD 206936 (M2Ia) Francois Ochsenbein CDS 1996 Sep 25 Catherine Boisson <boisson@obspm.fr> J_A+AS_117_93.xml Photographic observations of Pluto 1991-1994 with the Baldone Schmidt telescope. J/A+AS/118/105 J/A+AS/118/105 Pluto 1991-1994 observations Photographic observations of Pluto 1991-1994 with the Baldone Schmidt telescope. V P Ryl'kov A A Dement'eva A Alksnis J I Straume Astron. Astrophys. Suppl. Ser. 118 105 1996 1996A&AS..118..105R Planets Positional data astrometry planets and satellites: individual (Pluto) 55 equatorial geocentric coordinates of Pluto from the photographic observations for 1991-1994 are presented in the table. The observations were carried out by Latvian astronomers using the 80/120/240 cm Schmidt telescope at Baldone near Riga. 34 plates were measured and the positions of Pluto were reduced by using the 12-21 reference stars from catalogue of southern stars FOCAT-S, created at Pulkovo. The mean reduction errors vary from 0.23" to 0.34" for both coordinates. The obtained Pluto positions were compared with the ephemeris JPL DE200 (the residuals (O-C) were calculated). The increase of the average annual (O-C) residuals in RA, already noticed in previous works by the Pulkovo authors, is confirmed. From observations, represented in 1994 the (O-C) residuals with respect to DE200 have reached in RA +2.32+/-0.07" and in Dec. -0.74+/-0.07". More detailed information on obtaining the Pluto positions is given in Ryl'kov (1993) and Ryl'kov et.al. (1993).
Equatorial geocentric coordinates of Pluto from the observations 1991-1994 with the Baldone Schmidt telescope. No Plate number, photographed with Schmidt telescope --- Date Observation date "DD/MM/YY" JD Julian day d RAh Right ascension J2000.0 h RAm Right ascension J2000.0 min RAs Right ascension J2000.0 s DE- Declination sign --- DEd Declination J2000.0 deg DEm Declination J2000.0 arcmin DEs Declination J2000.0 arcsec DRA Residuals (O-C) in RA s DDE Residuals (O-C) in DE arcsec Obs Abbreviations of observer names number=1 Observers with the Baldone Schmidt telescope: Al. - A.Alksnis, Eg. - I.Eglitis, Jr. - I.Jurgitis, Pu. - I.Pundure, St. - J.I.Straume. --- Patricia Bauer CDS 1996 Apr 01 J_A+AS_118_105.xml Optical and I-band surface photometry of spiral galaxies. I. The data J/A+AS/118/111 J/A+AS/118/111 BVRI photometry of 234 spiral galaxies Optical and I-band surface photometry of spiral galaxies. I. The data P Heraudeau F Simien Astron. Astrophys. Suppl. Ser. 118 111 1996 1996A&AS..118..111H Galaxies, photometry Radial velocities galaxies: photometry galaxies: spiral We present V- and I-band CCD surface photometry on 234 inclined Sa-Sd galaxies, completed by similar data in B and R for a reduced subsample. In this first paper of a series, the reduction of the data is discussed, and several comparisons are made with other recent works. Radial profiles are presented for the surface brightness and the characteristics of ellipses fitted to isophotes; global, effective, and isophotal parameters are listed.
Catalog elements No Sequence number --- Name Object identification --- T Coded morphological type --- MType =XXXX Full morphological type --- RAh Right Ascension 1995 (hours) number=2 the equinox was erroneously indicated as 1950 in the original table; it was corrected into 1995 in February 1997. h RAm Right Ascension 1995 (minutes) number=2 the equinox was erroneously indicated as 1950 in the original table; it was corrected into 1995 in February 1997. min RAs Right Ascension 1995 (seconds) number=2 the equinox was erroneously indicated as 1950 in the original table; it was corrected into 1995 in February 1997. s DE- Declination 1995 (sign) number=2 the equinox was erroneously indicated as 1950 in the original table; it was corrected into 1995 in February 1997. --- DEd Declination 1995 (degrees) number=2 the equinox was erroneously indicated as 1950 in the original table; it was corrected into 1995 in February 1997. deg DEm Declination 1995 (minutes) number=2 the equinox was erroneously indicated as 1950 in the original table; it was corrected into 1995 in February 1997. arcmin DEs Declination 1995 (seconds) number=2 the equinox was erroneously indicated as 1950 in the original table; it was corrected into 1995 in February 1997. arcsec Bt Integrated B magnitude mag D25 Apparent diameter at brightness mu_B=25 arcmin Eps Ellipticity at brightness mu_B=25 --- HRV Heliocentric radial velocity km/s -Mb Absolute B magnitude (sign reversed) number=1 Absolute B magnitude determined from Bt corrected for Galactic extinction, and from radial velocity corrected corrected for Virgocentric infall, with H0=75 km/s/Mpc (see Sect. 2.1); when the corrected V_helio is smaller than 500 km/s, however, we adopted a distance modulus relying on other parameters provided by LEDA: this is the case for NGC 762, NGC 2976, and NGC 6503. mag S Sample --- Observation log Name Object identification --- m_Name Multiplicity index on Name --- Filt Photometric filter (B, V, R, or I) --- Exp Exposure time s Seeing Seeing FWHM arcsec Run Date of observing run (Month Year) --- Notes Notes --- Photometric results No Sequence number --- Name Object identification --- PA Major-axis position angle (North --> East) deg Eps Isophote ellipticity number=1 Determined as specified by parameter C --- n_Eps Code for the determination of Epsilon number=2 C=1: measurement in I at mu_I=23.5mag/arcsec2; C=2: in V at mu_V=24mag/arcsec2; C=3: in I at mu_I=22mag/arcsec2; C=4: in I at mu_I=21mag/arcsec2 --- Filt Photometric filter (B, V, R or I) --- TMag Total magnitude mag e_TMag rms error on TMag mag re Semi-major axis of the effective isophote arcsec e_re rms error on re arcsec mue Surface brightness at re (/ sq. arcsec) mag/arcsec2 e_mue rms error on mue mag/arcsec2 Diso Isophotal diameter number=3 Major axis of isophote mu_B=25mag/arcsec2, or mu_V=24mag/arcsec2, or mu_R=24mag/arcsec2, or mu_I=23.5mag/arcsec2 arcsec e_Diso rms error on Diso arcsec Q Quality parameter (Sect. 3.2) --- Photometric profiles in B, V, R, and/or I for 234 galaxies Name Object identification --- Rad Semi-major axis arcsec PA Position angle deg Eps Ellipticity --- muB Surface brightness/sq.arcsec, in B mag/arcsec2 e_muB rms error on muB mag/arcsec2 muV Surface brightness/sq.arcsec, in V mag/arcsec2 e_muV rms error on muV mag/arcsec2 muR Surface brightness/sq.arcsec, in R mag/arcsec2 e_muR rms error on muR mag/arcsec2 muI Surface brightness, in I mag/arcsec2 e_muI rms error on muI mag/arcsec2 Heraudeau & Simien CRAL Patricia Bauer CDS 1996 May 31 Philippe Heraudeau <ph@cumulus.univ-lyon1.fr> UNKNOWN UNKNOWN * 28-Feb-1997: the equinox of positions in table2 was fixed from 1950 to 1995.0 (error confirmed by Philippe Heraudeau) J_A+AS_118_111.xml Studies of dense molecular cores in regions of massive star formation. IV. Multitransition CS-study towards southern H_2_O masers in the longitude range l=308-360deg J/A+AS/118/191 J/A+AS/118/191 Multitransition CS-study towards H2O masers Studies of dense molecular cores in regions of massive star formation. IV. Multitransition CS-study towards southern H_2_O masers in the longitude range l=308-360deg M Juvela Astron. Astrophys. Suppl. Ser. 118 191 1996 1996A&AS..118..191J Masers Radial velocities Radio lines ISM: clouds ISM: molecules masers radio lines: ISM stars: formation We have observed CS and C^34^S emission towards 33 H_2_O maser positions in the southern sky ({delta}<-28deg) using the SEST telescope. Most of the sources were selected also for their association with strong IRAS sources. CS(2-1) was detected in all sources, with the possible exception of two. Most sources were also mapped in the transitions CS(5-4) and C^34^S(2-1) and half of the sample also in CS(2-1). CS and C^34^S transitions J=2-1, J=3-2 J=5-4 were measured towards the centres of the clouds as determined from the mapping. CS and C^34^S transitions J=7-6 were measured in about a half dozen clouds. CO(1-0) was measured in most clouds in order to determine the kinetic temperatures. The CS column densities were calculated using the LTE approximation. All measurements were also analyzed using a spherical LVG model. We present the observational data and the results of this analysis.
The source list Name Source name --- names Other names --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec RV Radial velocity of the H2O maser km/s n_RV A '+' indicates velocity of an OH maser --- DistG Galacto-centric distance kpc Dist1 Kinematic distance from CS data kpc u_Dist1 Uncertainty flag on Dist1 --- Dist2 Kinematic distance from C^34^S data kpc u_Dist2 Uncertainty flag on Dist2 --- z1 Height above the galactic plane from CS data pc u_z1 Uncertainty flag on z1 --- z2 Height above the galactic plane from C^34^S data pc u_z2 Uncertainty flag on z2 --- DistRef Distance estimates from the literature kpc r_DistRef Distance references number=1 Distance references: 1. Caswell J.L. & Haynes R.F. 1987, A&A, 171, 261 =1987A&A...171..261C 2. Henning T. et al. 1990, A&A, 227, 542 =1990A&A...227..542H 3. Lockman F. 1979,ApJ, 232, 761 =1979ApJ...232..761L 4. Moorwood A.F.M. et al. 1983, A&A, 125, 342 =1983A&A...125..342M 5. Neckel T. et al. 1978, A&A, 69, 51 =1978A&A....69...51N 6. Simpson J.P. et al. 1990, ApJ, 354, 165 =1990ApJ...354..165S 7. Testi L. et al. 1994, A&A, 288, 634 =1994A&A...288..634T 8. Zavagno A. et al. 1992, A&A, 259, 241 =1992A&A...259..241Z --- Ref Maser references number=2 Maser references: a. Batchelor R.A. et al. 1980, Aust. J. Phys., 33, 139 =1980AuJPh..33..139B b. Braz M.A. & Scalise E. Jr. 1982, A&A, 107, 272 =1982A&A...107..272B c. Braz M.A. et al. 1989, A&AS, 77, 465 =1989A&AS...77..465B d. Caswell J.L. et al. 1983, Aust. J. Phys., 36, 401 =1983AuJPh..36..361C e. Forster J.R. & Caswell J.L. 1989, A&A, 213, 339 =1989A&A...213..339F f. Guesten R. & Downes D. 1983, A&A, 117, 343 =1983A&A...117..343G g. Kaufmann P. et al. 1977, AJ, 82, 577 =1977AJ.....82..577K h. Moran J.M. & Rodriguez L.F. 1980, ApJ, 236, L159 =1980ApJ...236L.159M i. Scalise E. Jr. & Braz M.A. 1980, A&A, 85, 149 =1980A&A....85..149S --- CS and C^34^S lines area and Gaussian line parameters for the central positions of the sources Name Source name --- Pos Offsets of the observed position relative to the positions given in table2 --- J J values for the upper level of each transition --- IntTmb1 Integrated line temperature (from C^34^S data) K.km/s e_IntTmb1 rms uncertainty on IntTmb1 K.km/s Tmb1 Line temperature (from C^34^S data) K e_Tmb1 rms uncertainty on Tmb1 K RV1 Radial velocity (from C^34^S data) km/s e_RV1 rms uncertainty on RV1 km/s DV1 Observed line width (from C^34^S data) km/s e_DV1 rms uncertainty on DV1 km/s wing1 Note on the spectra number=1 b: blue wing, r: red wing, a: strong absorption --- IntTmb2 Integrated line temperature (from CS data) K.km/s e_IntTmb2 rms uncertainty on IntTmb2 K.km/s Tmb2 Line temperature (from CS data) K e_Tmb2 rms uncertainty on Tmb2 K RV2 Radial velocity (from CS data) km/s e_RV2 rms uncertainty on RV2 km/s DV2 Observed line width (from CS data) km/s e_DV2 rms uncertainty on DV2 km/s wing2 Note on the spectra number=1 b: blue wing, r: red wing, a: strong absorption --- wing3 Note on the spectra number=1 b: blue wing, r: red wing, a: strong absorption --- Results for the LTE analysis of the CS observations Name Source name --- J J values for the upper level of each transition --- Tex Excitation temperature K e_Tex rms uncertainty on Tex K taup Optical depth from C^34^S data (classical method) number=1 The optical depth tau_p_ was obtained in the usual manner from the ratio of the peak main beam temperatures assuming identical excitation temperatures and beam filling factors for both isotopes. --- e_taup rms uncertainty on taup --- taua Optical depth from C^34^S data (second method) number=2 If one takes into account the line broadening due to the optical depth (Phillips et al., =1979ApJ...231..720P), the observed line width, DV, can be expressed in terms of the line width of the optically thin line, DV0, as DV=(DV0/sqrt(ln2)).sqr(ln(tau/ln[2/1+exp(-tau)])). This expression can be used to derive the optical depth from the ratio of the line area for the two isotopes. This value of the optical depth is denoted tau_a_. --- e_taua rms uncertainty on taua --- log(N) Column density calculated from the line integrals (C^34^S data) cm-2 e_log(N) rms uncertainty on log(N) cm-2 The densities and cloud masses calculated in LTE approximation from the lines C^34^S(2-1) and CS(2-1) Name Source name --- Dist Distance kpc Size Size arcsec log(n) Density cm-3 Mass Cloud mass solMass Mvir Virial mass of the core solMass Results from the LVG analysis Name Source name --- Tkin Kinetic temperature K u_Tkin Uncertainty flag on Tkin --- l_log(n1) Limit flag on log(n1) --- log(n1) Total gas density derived from CS data cm-3 e_log(n1) rms uncertainty on log(n1) 0.1cm-3 log(N1) ^32^CS column density (from CS data) cm-2 log(n2) Total gas density derived from C^34^S data cm-3 e_log(n2) rms uncertainty on log(n2) 0.1cm-3 log(N2) ^32^CS column density (from C^34^S data) cm-2 e_log(N2) rms uncertainty on log(N2) 0.1cm-2 Patricia Bauer CDS 1996 Apr 04 J_A+AS_118_191.xml First catalogue of stars with photoelectric astrolabe in San Juan J/A+AS/118/1 J/A+AS/118/1 CPASJ1 catalogue First catalogue of stars with photoelectric astrolabe in San Juan L Lu W T Manrique R Perdomo R C Podesta Z Wang E L Actis F Zeng Z Zeng E Alonso A Serafino G Zhao J Hormaechea Astron. Astrophys. Suppl. Ser. 118 1 1996 1996A&AS..118....1L Magnitudes Positional data Spectral types astrometry catalogs reference systems On the basis of the data observed with the photoelectric astrolabe Mark II(PA II) of Beijing Astronomical Observatory in San Juan of Argentina from Feb. 23, 1992 to Feb. 28, 1995, residuals of 7200 stars are reduced according to about 230000 observations of stars. The mean precision of the residuals is +/-0.046". Using the data, the first catalogue of stars (CPASJ1) have been compiled. There are 2980 stars in this catalogue included 989 FK5/FK4Supp stars, 658 FK5Ext stars, 387 SRS stars, 687 CAMC4 stars, 192 GC stars, and 72 Hipparcos stars. The mean precisions are +/-3.2ms and +/-0.061" in right ascensions and declinations, respectively. The magnitudes of stars are from 2mag to 11.3mag. The declinations are from -3deg to -60deg. The mean epoch is 1993.6. Finally, systematic corrections of(CPASJ1-FK5) are given.
First Catalogue of Stars with Photoelectric Astrolabe in San Juan CPASJ1 This catalogue reference number --- No Catalogues number number=1 FK5 (No 1 to 467) or FK4Supp (468-989) or FK5Ext (990-1647) or SRS (1648-2034) or CAMC4 (2035-2715) or GC (2716-2908) or Hipparcos (2909-2980) number --- Vmag Visual magnitude mag Sp Spectral type --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s pmRA Proper motion in RA (J2000.0) s/ha DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec DRA Position correction on right ascension ms pmDE Proper motion in DE (J2000.0) arcsec/ha e_DRA rms uncertainty on DRA ms DDE Position correction on declination 0.01arcsec e_DDE rms uncertainty on DDE 0.01arcsec Ne Eastern transit number of observations --- Nw Western transit number of observations --- Epoch Mean epoch of observation yr catalog.tex LaTeX version of the catalogue Patricia Bauer CDS 1996 Mar 15 J_A+AS_118_1.xml Radial velocities and axial rotation of a sample of chemically peculiar stars. J/A+AS/118/231 J/A+AS/118/231 Velocities & rotation of CP stars Radial velocities and axial rotation of a sample of chemically peculiar stars. H Levato S Malaroda N Morrell G Solivella M Grosso Astron. Astrophys. Suppl. Ser. 118 238 1996 1996A&AS..118..231L Radial velocities Rotational velocities Stars, peculiar stars: chemically peculiar stars: kinematics stars: rotation As part of a systematic project we have determined radial velocities and projected rotational velocities for a sample of 186 chemically peculiar stars which have been observed by the Hipparcos' satellite. The purpose is to provide necessary data to study the space velocities of peculiar stars.
Individual observations HD HD number --- JD Julian Date of the observation d RV Radial velocity km/s e_RV Probable error of the observation km/s N Number of spectral lines including in the average of radial velocity --- Statistical results HD HD number --- RV Average radial velocity km/s e_RV Probable error on radial velocity km/s N Number of spectra included in the average --- Ext.e_RV External probable error km/s Int.e_RV Internal probable error km/s E/I Quotient between the external and internal errors --- l_Prob Limit flag on Prob --- Prob Probability (or upper value if n_Prob = '-') that the sample of radial velocities was drawn from a random population % n_Prob A '-' indicates an interval --- Prob2 Lower value of the probability when n_Prob='-' % l_vsini Limit flag on vsini --- vsini Axial rotation km/s Sp Spectral classification --- Patricia Bauer CDS 1996 Apr 10 J_A+AS_118_231.xml The photoelectric astrolabe catalogue of Yunnan Observatory (YPAC) J/A+AS/118/239 J/A+AS/118/239 Yunnan Observatory photoelectric astrolabe catalogue The photoelectric astrolabe catalogue of Yunnan Observatory (YPAC) H Hu D Li Y Li R Wang X Li Astron. Astrophys. Suppl. Ser. 118 239 1996 1996A&AS..118..239H I/149 : Fifth Fundamental Catalogue (FK5) I/175 : Fifth Fundamental Catalogue (FK5) - Extension I/113 : General Catalogue of 33342 stars (GC) Fundamental catalog Positional data catalogs The positions of 53 FK5, 70 FK5 Extension and 486 GC stars are given for equator and the equinox J2000.0 and for the mean observation epoch of each star which are determined with the photoelectric astrolabe of Yunnan Observatory. The internal mean errors in right ascension and declination are 0.046" and 0.059", respectively. The mean observation epoch is 1989.51.
J2000 positions of YPAC YPAC Number in YPAC --- Catal Catalogue's designation number=1 Name from FK5-Fifth Fundamental Catalogue; EXT-FK5 Extension or GC-Boss General Catalogue. --- Vmag Visual magnitude from above catalogue. mag RAh Right ascension J2000.0 h RAm Right ascension J2000.0 min RAs Right ascension J2000.0 s DE- Declination sign --- DEd Declination J2000.0 deg DEm Declination J2000.0 arcmin DEs Declination J2000.0 arcsec n_RAs Internal precision of right ascension. ms n_DEs Internal precision of declination. 10mas Mean epoch of observations minus 1900.00. yr DRA Differences YPAC-FK5 or YPAC-CMC in RA ms DDE Differences YPAC-FK5 or YPAC-CMC in DE 10mas Name Number of FK5 or CMC, where the one that is larger than 10000 is that of the CMC. number=2 These stars are used to calculate the external accuracy of YPAC. When the number in YPAC larger than 221, bytes 57-70 are blank, since these stars all are GC stars of non-FK5 or non-CMC. --- Patricia Bauer CDS 1996 Jun 28 J_A+AS_118_239.xml The astrometric accuracy of ``Carte du Ciel'' plates and proper motions in the field of the open cluster NGC 1647 J/A+AS/118/277 J/A+AS/118/277 Proper motions in NGC 1647 The astrometric accuracy of ``Carte du Ciel'' plates and proper motions in the field of the open cluster NGC 1647 M Geffert P Bonnefond G Maintz J Guibert Astron. Astrophys. Suppl. Ser. 118 277 1996 1996A&AS..118..277G Clusters, open Proper motions astrometry open clusters and associations: individual (NGC 1647) stars: individual (SZ Tau) The astrometric accuracy of triple image Carte du Ciel plates has been analysed using plates of the open cluster NGC 1647. A new multithreshold technique was used for the treatment of the triple image plates. Accuracies ranging from 100mas to 200mas were found. We determined proper motions with a median accuracy of 1.6mas/a for 2220 stars in the field of NGC 1647. The membership probabilities of stars in the cluster region agree very well with the data of Francic (1989). Due to a significant difference of the proper motions of SZ Tau and the cluster members, SZ Tau seems not to be a member of NGC 1647.
Positions and proper motions of 2220 stars in the region of NGC 1647. NR Internal star number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec pmRA Proper motion in right ascension mas/a pmDE Proper motion in declination mas/a Patricia Bauer CDS 1996 Sep 16 Michael Geffert <geffert@astro.uni-bonn.de> J_A+AS_118_277.xml Variable stars in the field of the old open cluster NGC 2243 J/A+AS/118/303 J/A+AS/118/303 VI Photometry of variables in NGC 2243 Variable stars in the field of the old open cluster NGC 2243 J Kaluzny W Krzeminski B Mazur Astron. Astrophys. Suppl. Ser. 118 330 1996 1996A&AS..118..303K Photometry, CCD Stars, variable binaries: close binaries: eclipsing open clusters and associations: individual (NGC 2243) stars: variables: other Tables 3-13 contain V and I band light curves for 6 variables reported in the paper. Tables 14 and 15 contain VI photometry presented in Figs. 5 and 9, respectively.
NGC 2243 06 29.8 -31 17
V-band light curve of variable V1 V-band light curve of variable V2 V-band light curve of variable V3 V-band light curve of variable V4 V-band light curve of variable V5 V-band light curve of variable V6 I-band light curve of variable V1 I-band light curve of variable V2 I-band light curve of variable V3 I-band light curve of variable V5 I-band light curve of variable V6 HJD Heliocentric Julian day -2440000 d Vmag V magnitude mag e_Vmag Error of Vmag mag *VI photometry for field of NGC2243, TEK2 data ID ID number --- Xpos X coordinate (toward South), 1 pixel=0.61 arcsec pix Ypos Y coordinate (toward East), 1 pixel=0.61 arcsec pix Vmag V magnitude mag e_Vmag Error of V mag V-I V-I color index mag e_V-I Error of V-I mag *VI photometry for field of NGC2243, TEK3 data ID ID number --- Xpos X coordinate (toward East), 1 pixel=0.61 arcsec pix Ypos Y coordinate (toward South), 1 pixel=0.61 arcsec pix Vmag V magnitude mag e_Vmag Error of V mag V-I V-I color index mag e_V-I Error of V-I mag Janusz Kaluzny ? 1996 Aug 22 J_A+AS_118_303.xml The MOST supernova remnant catalogue (MSC). J/A+AS/118/329 J/A+AS/118/329 MOST supernova remnant catalogue The MOST supernova remnant catalogue (MSC). J B Z Whiteoak A J Green Astron. Astrophys. Suppl. Ser. 118 329 1996 1996A&AS..118..329W VII/210 : A Catalogue of Galactic Supernova Remnants (Green, 1996) VII/15 : Galactic supernova remnants catalog (Ilovaisky+ 1972) VII/14 : Galactic supernova remnants catalog (Clark+ 1979) Morphology Radio lines Supernova remnants atlases catalogs radio continuum: ISM supernova remnants surveys A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}<=l<=355{deg}, |b|<~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).
Parameters of known, new, possible SNRs Status Known. New, Possible or Rejected SNR this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- NoteFlag indicates a note in file notes.dat number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- MSC Supernova remnant name (GLLL.l+B.b) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- RAh Right ascension (J2000.0) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W h RAm Right ascension (J2000.0) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W min RAs Right ascension (J2000.0) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W s DE- Declination sign number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- DEd Declination (J2000.0) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W deg DEm Declination (J2000.0) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W arcmin DEs Declination (J2000.0) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W arcsec l_S0.843 Limit flag on S0.843 number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- S0.843 Integrated flux density at 0.843GHz number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W Jy DMaj Major diameter at 0.843GHz number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W arcmin --- number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- DMin Minor diameter at 0.843GHz number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W arcmin l_SB0.843 Limit flag on SB0.843 number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- SB0.843 Mean surface brightness at 0.843GHz number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W 10+5Jy/sr Type Type S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure --- Fig Figure number (not for possible SNR) number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- RefMOST Reference to previous MOST publications references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- Remarks Remarks, including common names and references number= this flag takes the values: k: Known SNR (Table MSC.A of the paper) n: New SNR (Table MSC.B of the paper) p: Possible SNR (Table MSC.C of the paper) r: Reclassifed (section 3.3 of the paper) number= S: shell P: plerion or filled-centre C: composite *: apparent multiple shell structure number= references (for known SNRs only): 1: Caswell et al., 19833MNRAS.204..915C 2: Caswell et al., 1983PASAu...5..227C 3: Caswell et al., 1992ApJ...399L.151C 4: Haynes, 1987AuJPh..40..741H 5: Kesteven & Caswell, 1987A&A...183..118K 6: Kesteven et al., 1987AuJPh..40..855K 7: Manchester & Durdin, 1983IAUS..101..421M 8: Milne et al., 1985PASAu...6...78M 9: Milne et al., 1988, in: Kundt W. (ed.) Supernova Shells and their Birth Events,. Spinger-Verlag, p.98 10: Milne et al., 1989PASAu...8..187M 11: Roger at al., 1985Natur.316...44R 12: Roger et al., 1986MNRAS.219..815R 13: Whiteoak et al., 1989PASAu...8..176W 14: Whiteoak, 1990Natur.347..157W 15: Whiteoak, 1992MNRAS.256..121W 16: Whiteoak, 1993ApJ...415..701W --- Individual notes MSC Object name (GLLL.l+B.b) --- Note Text of the note --- James Marcout, Patricia Bauer, Francois Ochsenbein CDS 1999 Feb 26 UNKNOWN UNKNOWN * 06-Oct-1998: Prepared via OCR at CDS. * 26-Feb-1999: tables merged into a single catalogue J_A+AS_118_329.xml Provisional orbits for three visual binaries J/A+AS/118/381 J/A+AS/118/381 COU 247, ADS 3672 & ADS 15182 observations Provisional orbits for three visual binaries D M D Jasinta Astron. Astrophys. Suppl. Ser. 118 381 1996 1996A&AS..118..381J Binaries, orbits Stars, double and multiple astrometry binaries: visual This paper presents new orbits for two visual double stars COU 247 (CCDM 00095+1907) and ADS 3672 (STT 95, CCDM 05055+1948) and a revised orbit for ADS 15182 (A 772, CCDM 21395+3009) computed by the Thiele-van den Bos method.
COU 247 CCDM 00095+1907 00 09.5 +19 07 ADS 3672 CCDM 05055+1948 05 05.5 +19 48 ADS 15182 CCDM 21395+3009 21 39.5 +30 09
Observations and residuals of COU 247, ADS 3672 and ADS 15182 Name Star name --- Date Epoch of observation yr theta Position angle deg n_theta Note on theta number=1 An * indicates that means positions have been rotated 180deg by the author --- rho Angular separation arcsec o_rho Number of observations --- Observer Observer name --- DPA (O-C) in position angle deg DSep (O-C) in angular separation arcsec Patricia Bauer CDS 1996 Apr 15 J_A+AS_118_381.xml Critical tests of stellar evolution in open clusters. I. New photometry and radial velocities for NGC 3680 J/A+AS/118/407 J/A+AS/118/407 CCD photometry & velocities of NGC 3680 stars Critical tests of stellar evolution in open clusters. I. New photometry and radial velocities for NGC 3680 B Nordstroem J Andersen M I Andersen Astron. Astrophys. Suppl. Ser. 118 407 1996 1996A&AS..118..407N Clusters, open Photometry, CCD Radial velocities Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 3680) stars: evolution stars: fundamental parameters stars: kinematics We present new CCD photometry in the b and y colours of the Stroemgren uvby system for 310 stars in a 13'x13' field centered on the intermediate-age open cluster NGC 3680. Careful cross-checks indicate that previously published BV photometry of NGC 3680 is affected by random and/or systematic errors precluding its use in critical comparison with theoretical isochrone computations. Detailed notes on several individual stars are given. In addition, we present =~400 new photoelectric radial-velocity observations of 109 stars obtained with the CORAVEL scanner during the period 1988-1994. These data allow substantially complete identification of member and non-member stars in the field, and of spectroscopic binaries in both groups. Rotational velocities have also been derived for the programme stars, and our velocity variability criteria for stars of all rotations are described. The further astrophysical discussion of the data, including the definition of radial-velocity membership criteria, theoretical isochrone fitting, and the dynamical state of the cluster and the origin of its "bimodal turnoff", will appear in a separate paper (Nordstroem et al. 1996).
Coordinates and CCD photometry for 352 stars in the field of NGC 3680 No Identification number from paper --- m_No Multiplicity index on No --- RAh Right Ascension (J2000) h RAm Right Ascension (J2000) min RAs Right Ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag b-y b-y color index in Stroemgren system mag Mean radial and rotational velocities and derived parameters for 109 stars in the field of NGC 3680 No Identification number from paper --- m_No Multiplicity index on No --- KP Number in Kozhurina-Platais et al. (1995) --- RV Mean radial velocity km/s e_RV Mean error of mean radial velocity km/s o_RV Number of radial-velocity observations --- sigmaO Observed standard deviation (one obs.) km/s sigmaP Predicted standard deviation (one obs.) km/s O/Psigma ratio observed/predicted standard deviations --- Prob Probability that radial velocity is constant --- RVtot =-9.99 total observed range in radial velocity km/s Obs Time span covered by observations d vsini mean projected rotational velocity km/s e_vsini Mean error of rotational velocity km/s Com Comments, M: Data from Mermilliod et al. (1995) *: See remark in paper itself --- Individual radial-velocity observation of the stars in table2 No Identification number from paper --- m_No Multiplicity index on No --- HJD Heliocentric Julian Date of observation d RV Radial velocity (for double-lined binaries: primary component data) km/s e_RV Predicted uncertainty of observed velocity km/s RV2 Radial velocity of the secondary component for double-lined binaries km/s e_RV2 Predicted uncertainty of observed velocity km/s tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Mar 18 J_A+AS_118_407.xml New aperture photometry for 217 galaxies in the Virgo and Fornax clusters. J/A+AS/118/441 J/A+AS/118/441 Virgo & Fornax clusters galaxies UBVRI data New aperture photometry for 217 galaxies in the Virgo and Fornax clusters. A Schroeder N Visvanathan Astron. Astrophys. Suppl. Ser. 118 441 1996 1996A&AS..118..441S Clusters, galaxy Photometry, UBVRI galaxies: clusters: individual (Virgo, Fornax) galaxies: photometry We present photoelectric multi-aperture photometry in UBVRI of 171 and 46 galaxies in the Virgo and Fornax clusters, respectively. Many of the galaxies have not been observed in at least one of these passbands before. We discuss the reduction and transformation into the Cousins photometric system as well as the extinction coefficients obtained between 1990 and 1993.
List of standard stars n_star * for stars observed with the S20 tube --- star Standard star name --- Vmag Standard V magnitude mag B-V Standard (B-V) magnitude mag DVmag Difference of our mean observed V magnitude and the standard value mag o_Vmag Number of useful observations --- D(U-B) Difference of our mean observed (U-B) colour and the standard value mag D(B-V) Difference of our mean observed (B-V) colour and the standard value mag D(V-R) Difference of our mean observed (V-R) colour and the standard value mag D(R-I) Difference of our mean observed (R-I) colour and the standard value mag o_UBVRI Number of useful observations of colours (can vary slightly from one colour to the next) --- Virgo and Fornax clusters aperture data No Identification of the galaxy by the number of the respective catalogue: VCC: Binggeli et al. =1985AJ.....90.1681B FCC: Ferguson et al. =1989AJ.....98..367F --- Name Name of the galaxy (NGC, IC, ESO, UGC or other identifications) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Mtype Morphological galaxy type (if available from VCC and FCC, else from RC3) --- Ap Aperture size arcsec logAp Logarithm of the aperture 0.1arcmin Rot Total integration time in units of rotations of the filter wheel(1) --- Bmag B magnitude mag n_Bmag Note on Bmag number=2 A colon indicates a signal-to-noise error of 0.10mag and more; bracket is used for data that has been excluded from further data reduction for various reasons, such as a) too low exposure times, b) exceptionally high sky counts (i.e., a large aperture), c) a bright star in the aperture was not measured or light from a star scattered into or out of the aperture, d) the aperture was not centered accurately, e) error too high. Sometimes only one or two passbands were affected. All data followed by bracket should be rejected. --- U-B U-B colour mag n_U-B Note on U-B number=2 A colon indicates a signal-to-noise error of 0.10mag and more; bracket is used for data that has been excluded from further data reduction for various reasons, such as a) too low exposure times, b) exceptionally high sky counts (i.e., a large aperture), c) a bright star in the aperture was not measured or light from a star scattered into or out of the aperture, d) the aperture was not centered accurately, e) error too high. Sometimes only one or two passbands were affected. All data followed by bracket should be rejected. --- B-V B-V colour mag n-B-V Note on B-V number=2 A colon indicates a signal-to-noise error of 0.10mag and more; bracket is used for data that has been excluded from further data reduction for various reasons, such as a) too low exposure times, b) exceptionally high sky counts (i.e., a large aperture), c) a bright star in the aperture was not measured or light from a star scattered into or out of the aperture, d) the aperture was not centered accurately, e) error too high. Sometimes only one or two passbands were affected. All data followed by bracket should be rejected. --- V-R V-R colour mag n_V-R Note on V-R number=2 A colon indicates a signal-to-noise error of 0.10mag and more; bracket is used for data that has been excluded from further data reduction for various reasons, such as a) too low exposure times, b) exceptionally high sky counts (i.e., a large aperture), c) a bright star in the aperture was not measured or light from a star scattered into or out of the aperture, d) the aperture was not centered accurately, e) error too high. Sometimes only one or two passbands were affected. All data followed by bracket should be rejected. --- R-I R-I colour mag n_R-I Note on R-I number=2 A colon indicates a signal-to-noise error of 0.10mag and more; bracket is used for data that has been excluded from further data reduction for various reasons, such as a) too low exposure times, b) exceptionally high sky counts (i.e., a large aperture), c) a bright star in the aperture was not measured or light from a star scattered into or out of the aperture, d) the aperture was not centered accurately, e) error too high. Sometimes only one or two passbands were affected. All data followed by bracket should be rejected. --- Notes Notes number=3 A star indicates if a star (or more than one star) was included in and subtracted from the aperture. S20 indicates that the aperture was observed with the S20 tube. Brackets after S20 indicate an aperture that was partly observed with the S20 and with the GaAs tube. --- table2.tex LaTeX version of table2 table5a.tex LaTeX version of table5, first part table5b.tex LaTeX version of table5, second part Patricia Bauer CDS 1996 Apr 30 Anja Schroeder <SCHROEDER1@ubaclu.unibas.ch> J_A+AS_118_441.xml Dust and CO emission in normal spirals. I. The data J/A+AS/118/47 J/A+AS/118/47 CO observations in spirals Dust and CO emission in normal spirals. I. The data R Chini E Kruegel R Lemke Astron. Astrophys. Suppl. Ser. 118 47 1996 1996A&AS..118...47C Carbon monoxide Galaxies, radio galaxies: abundances galaxies: ISM galaxies: spiral radio continuum: galaxies radio lines: galaxies We present 1300{mu}m continuum observations and measurements of the CO (1-0) and (2-1) emission from the inner regions of 98 normal galaxies. The spatial resolution ranges from 11arcsec to 45arcsec. The sources come from a complete FIR selected sample of 138 inactive spirals with an optical diameter D_25_<=180arcsec.
Dust emission in normal spirals Name Galaxy name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Dist Distance Mpc S11 1300um flux density whithin 11" area, IRAM 30m telescope (MRT) observations mJy e_S11 rms uncertainty on S11 mJy S24 1300um flux density whithin 24" area, Swedish ESO Submillimeter Telescope (SEST) observations mJy e_S24 rms uncertainty on S24 mJy S70 1300um flux density whithin 70" area, SEST observations mJy e_S70 rms uncertainty on S70 mJy CO emission in normal spirals Name Galaxy name --- n_Name A '*' indicates that the spectrum has been fitted by two Gaussians, and that the followed data are from the second Gaussian --- Vc1 CO(1-0) MRT (24") central velocity km/s dVc1 CO(1-0) MRT (24") line width km/s Tmb1 CO(1-0) MRT (24") temperature mK Vc2 CO(1-0) SEST (45") central velocity km/s dVc2 CO(1-0) SEST (45") line width km/s Tmb2 CO(1-0) SEST (45") temperature mK Vc3 CO(2-1) MRT (12") central velocity km/s dVc3 CO(2-1) MRT (12") line width km/s Tmb3 CO(2-1) MRT (12") temperature mK Vc4 CO(2-1) SEST (24") central velocity km/s dVc4 CO(2-1) SEST (24") line width km/s Tmb4 CO(2-1) SEST (24") temperature mK I24" I(2-1)/(1-0) integrated intensities ratio with the (1-0) lines coming from the 30m telescope and the other from SEST --- ISEST I(2-1)/(1-0) integrated intensities ratio observations refers to 45" in the (1-0) transition and 24" in (2-1) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Apr 02 J_A+AS_118_47.xml The ROSAT all-sky survey catalogue of optically bright OB-type stars. J/A+AS/118/481 J/A+AS/118/481 ROSAT all-sky survey catalogue of OB stars The ROSAT all-sky survey catalogue of optically bright OB-type stars. T W Berghoefer J H M M Schmitt J P Cassinelli Astron. Astrophys. Suppl. Ser. 118 481 1996 1996A&AS..118..481B V/50 : The Bright Star Catalogue IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) Stars, OB X-ray sources stars: early-type X-rays: stars For the detailed statistical analysis of the X-ray emission of hot stars we selected all stars of spectral type O and B listed in the Yale Bright Star Catalogue and searched for them in the ROSAT All-Sky Survey. In this paper we describe the selection and preparation of the data and present a compilation of the derived X-ray data for a complete sample of bright OB stars.
ROSAT
Detections HR Bright Star catalogue number --- Name Star's name --- SpType MK spectral classification --- Vmag V magnitude mag B-V B-V magnitude mag E(B-V) Color excess mag log(NH) Hydrogen column density cm-2 Dist Distance pc log(Lbol) Bolometric luminosity 10-7W Texp Exposure time s OX-sep Offset between optical and X-ray position arcsec n_OX-sep * for offset larger than 75 arcmin --- rate Mean PSPC count rate ct/s e_rate Error of PSPC count rate ct/s HRatio Hardness ratio = (H-S)/(H+S) --- e_HRatio Error of hratio --- n_HRatio Note on hardness ratio -: up. limit +: low. limit 1: only S band --- Tx Estimated X-ray temperature keV log(FX) Apparent X-ray flux mW/m2 log(e_FX) Error of FX mW/m2 log(Lx) X-ray luminosity 10-7W log(Lx/Lbol) Luminosity ratio log(Lx/Lbol) --- Upper limits of non-detections HR Bright Star catalogue number --- SpType MK spectral classification --- Vmag V magnitude mag log(Lx) Upper limit for X-ray luminosity 10-7W Lx-Lbol Upper limit for luminosity ratio log(Lx/Lbol) --- Patricia Bauer CDS 1996 Apr 25 J_A+AS_118_481.xml Proper motions of stars in the region of the Orion Nebula cluster (C 0532-054) J/A+AS/118/503 J/A+AS/118/503 Proper motions of stars in Ori Nebula Proper motions of stars in the region of the Orion Nebula cluster (C 0532-054) K P Tian F Van Leeuwen J -L Zhao C G Su Astron. Astrophys. Suppl. Ser. 118 503 1996 1996A&AS..118..503T II/171 : PARENAGO Catalogue of stars in the area of the Orion Nebula Parenago, P.P. 1954, Trudy Sternberg Astron.Inst. Vol.25 =Catalogue <II/171> Clusters, open Proper motions astrometry open clusters and associations: general open clusters and associations: individual (C 0532-054) Relative proper motions and membership probabilities for 333 stars within an area of 1.6deg by 1.8deg centred on the Orion Nebula M 42 are determined using plates taken over a period of 83 years with the double astrograph of Shanghai Observatory (scale of 30"/mm). The plates were measured with the ASTROSCAN automatic plate-measuring machine of Leiden Observatory. The average proper motion accuracy obtained for stars in the photographic magnitude range 7 to 14 is 0.3mas/yr. Errors are somewhat larger towards fainter and brighter magnitude, but the majority lie well below 1mas/yr. 64% of the stars have been measured successfully on at least 13 out of 18 plates. The number of stars with membership probabilities higher than 0.7 is 184. It is shown by a detailed discussion that the proper motions and membership probabilities of the stars determined in this paper are in good agreement with the results presented recently by other authors. Although there is a clear concentration in the proper motion diagram, both the remaining dispersion of the internal motions and the distribution of "members" as projected on the sky indicate that the stars in this region are not bound as one system, but do have a common origin. A similar conclusion can be drawn from a comparison with spectroscopic and radial velocity data.
C 0532-054 M 42 Ori Nebula 05 35.4 -05 23
Results of the astrometric study No Sequential number --- Parenago Parenago number (Catalogue <II/171>) --- Pmag Photographic magnitude mag RAh Right ascension (J2000, Epoch 1950) h RAm Right ascension (J2000, Epoch 1950) min RAs Right ascension (J2000, Epoch 1950) s e_RAs rms uncertainty on RA ms DE- Declination sign --- DEd Declination (J2000, Epoch 1950) deg DEm Declination (J2000, Epoch 1950) arcmin DEs Declination (J2000, Epoch 1950) arcsec e_DEs rms uncertainty on DE mas pmRA Proper motion along RA mas/yr e_pmRA rms uncertainty on proper motion RA mas/yr pmDE Proper motion in DE mag/yr e_pmDE rms uncertainty on proper motion DE mag/yr Plate Number of plates used --- Ep-1950 Mean epoch in years, relative to 1950.0 yr Memb Membership probability in percents % Patricia Bauer CDS 1996 May 06 J_A+AS_118_503.xml Rotational velocities of F dwarfs; application of the Fourier-Bessel transformation method J/A+AS/118/545 J/A+AS/118/545 Rotational velocities of F dwarfs Rotational velocities of F dwarfs; application of the Fourier-Bessel transformation method P J Groot A J M Piters J van Paradijs Astron. Astrophys. Suppl. Ser. 118 545 1996 1996A&AS..118..545G III/63 : Revised Catalogue of Rotational Velocities (Uesugi+ 1982) Uesugi A. & Fukuda I., 1981, Proc. 7th CODATA Conf =Catalogue <III/63B> Bright star Catalogue (HR) =Catalogue <V/50> Slettebak A., 1955, ApJ 121, 653 =1955ApJ...121..653S Soderblom D.R., 1982, ApJ 263, 239 =1982ApJ...263..239S Rotational velocities Stars, F-type line: profiles stars: rotation techniques: spectroscopic table4 contains rotational velocities for 177 dwarfs with spectral types between A7 en G2.
Observed stars B-V colours, spectral type and rotational velocities HR HR Bright Star number of the star --- m_HR Multiplicity index for binary --- n_HR A 'a' indicates binary of which both lines were seen --- B-V B-V colour mag Sp Spectral type --- l_vsini1 Limit flag on vsini1 --- vsini1 Projected equatorial rotational velocity as determined with the Fourrier-Bessel transformation (FBT) method km/s e_vsini1 rms uncertainty on vsini1 km/s vsini2 Projected equatorial rotational velocity as determined with the convolution method km/s e_vsini2 rms uncertainty on vsini2 km/s l_vsini3 Limit flag on vsini3 --- vsini3 Projected equatorial rotational velocity as listed in the Bright Star Catalogue km/s vsini4 Projected equatorial rotational velocity as determined by Soderblom or Slettebak km/s n_vsini4 'sl' indicates Slettebak data --- l_vsini5 Limit flag on vsini5 --- vsini5 Projected equatorial rotational velocity as listed in catalogue of Uesugi and Fukuda km/s u_vsini5 Uncertainty flag on vsini5 --- N Number of lines used in determination of rotational velocity with the FBT method --- table4.tex LaTeX version of table4 Patricia Bauer CDS 1996 Apr 11 Paul Groot <paulgr@astro.uva.nl> J_A+AS_118_545.xml Near-infrared and optical broadband surface photometry of 86 face-on disk dominated galaxies. II. A two-dimensional method to determine bulge and disk parameters. J/A+AS/118/557 J/A+AS/118/557 Near-IR photometry of 86 galaxies. II. Near-infrared and optical broadband surface photometry of 86 face-on disk dominated galaxies. II. A two-dimensional method to determine bulge and disk parameters. R S De Jong Astron. Astrophys. Suppl. Ser. 118 557 1996 1996A&AS..118..557D J/A+A/313/377 : Near-IR photometry of 86 galaxies. IV. (de Jong 1996) Galaxies, photometry galaxies: fundamental parameters galaxies: photometry galaxies: spiral galaxies: structure methods: data analysis surveys In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong & van der Kruit (1994), which comprises 86 galaxies in six passbands.
List of galaxies RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin UGC Name of galaxy in UGC <VII/26> --- Names Other names --- Photometry information for the different passbands UGC Name of galaxy in UGC <VII/26> --- QBmag =-999 Q parameter for B band number=1 Q parameter as in thesis 1: photometric 2: 0.0-0.2 mag error 3: 0.2-0.5 4: 0.5-1.0 5: >1.0 -999 not available in this passband --- QVmag =-999 Q parameter for V band number=1 Q parameter as in thesis 1: photometric 2: 0.0-0.2 mag error 3: 0.2-0.5 4: 0.5-1.0 5: >1.0 -999 not available in this passband --- QRmag =-999 Q parameter for R band number=1 Q parameter as in thesis 1: photometric 2: 0.0-0.2 mag error 3: 0.2-0.5 4: 0.5-1.0 5: >1.0 -999 not available in this passband --- QImag =-999 Q parameter for I band number=1 Q parameter as in thesis 1: photometric 2: 0.0-0.2 mag error 3: 0.2-0.5 4: 0.5-1.0 5: >1.0 -999 not available in this passband --- QHmag =-999 Q parameter for H band number=1 Q parameter as in thesis 1: photometric 2: 0.0-0.2 mag error 3: 0.2-0.5 4: 0.5-1.0 5: >1.0 -999 not available in this passband --- QKmag =-999 Q parameter for K band number=1 Q parameter as in thesis 1: photometric 2: 0.0-0.2 mag error 3: 0.2-0.5 4: 0.5-1.0 5: >1.0 -999 not available in this passband --- Decompositions using the 2D technique, exponential bulge and Freeman bar UGC Name of galaxy in UGC <VII/26> --- Bfcs Central surface brightness of the disk mag/arcsec+2 e_Bfcs Formal fit error in Bfcs (real uncertainty in general much larger) mag/arcsec+2 Bfsc Scale length of disk arcsec e_Bfsc Formal fit error in Bfsc arcsec Bfes Central! (not effective) surface brightness of bulge mag/arcsec+2 e_Bfes Formal fit error in Bfes mag/arcsec+2 Bfer Bulge scale length (not effective radius) arcsec e_Bfer Formal fit error in Bfer arcsec Bfbc Central brightness of the bar mag/arcsec+2 e_Bfbc Formal fit error in Bfbc mag/arcsec+2 Bfma Bar major axis arcsec e_Bfma Formal fit error in Bfma arcsec Bfmi Bar minor axis arcsec e_Bfmi Formal fit error in Bfmi arcsec Bfpa Position angle of the bar deg e_Bfpa Formal fit error in Bfpa deg Vfcs Central surface brightness of the disk mag/arcsec+2 e_Vfcs Formal fit error in Vfcs (real uncertainty in general much larger) mag/arcsec+2 Vfsc Scale length of disk arcsec e_Vfsc Formal fit error in Vfsc arcsec Vfes Central! (not effective) surface brightness of bulge mag/arcsec+2 e_Vfes Formal fit error in Vfes mag/arcsec+2 Vfer Bulge scale length (not effective radius) arcsec e_Vfer Formal fit error in Vfer arcsec Vfbc Central brightness of the bar mag/arcsec+2 e_Vfbc Formal fit error in Vfbc mag/arcsec+2 Vfma Bar major axis arcsec e_Vfma Formal fit error in Vfma arcsec Vfmi Bar minor axis arcsec e_Vfmi Formal fit error in Vfmi arcsec Vfpa Position angle of the bar deg e_Vfpa Formal fit error in Vfpa deg Rfcs Central surface brightness of the disk mag/arcsec+2 e_Rfcs Formal fit error in Rfcs (real uncertainty in general much larger) mag/arcsec+2 Rfsc Scale length of disk arcsec e_Rfsc Formal fit error in Rfsc arcsec Rfes Central! (not effective) surface brightness of bulge mag/arcsec+2 e_Rfes Formal fit error in Rfes mag/arcsec+2 Rfer Bulge scale length (not effective radius) arcsec e_Rfer Formal fit error in Rfer arcsec Rfbc Central brightness of the bar mag/arcsec+2 e_Rfbc Formal fit error in Rfbc mag/arcsec+2 Rfma Bar major axis arcsec e_Rfma Formal fit error in Rfma arcsec Rfmi Bar minor axis arcsec e_Rfmi Formal fit error in Rfmi arcsec Rfpa Position angle of the bar deg e_Rfpa Formal fit error in Rfpa deg Ifcs Central surface brightness of the disk mag/arcsec+2 e_Ifcs Formal fit error in Ifcs (real uncertainty in general much larger) mag/arcsec+2 Ifsc Scale length of disk arcsec e_Ifsc Formal fit error in Ifsc arcsec Ifes Central! (not effective) surface brightness of bulge mag/arcsec+2 e_Ifes Formal fit error in Ifes mag/arcsec+2 Ifer Bulge scale length (not effective radius) arcsec e_Ifer Formal fit error in Ifer arcsec Ifbc Central brightness of the bar mag/arcsec+2 e_Ifbc Formal fit error in Ifbc mag/arcsec+2 Ifma Bar major axis arcsec e_Ifma Formal fit error in Ifma arcsec Ifmi Bar minor axis arcsec e_Ifmi Formal fit error in Ifmi arcsec Ifpa Position angle of the bar deg e_Ifpa Formal fit error in Ifpa deg Hfcs Central surface brightness of the disk mag/arcsec+2 e_Hfcs Formal fit error in Hfcs (real uncertainty in general much larger) mag/arcsec+2 Hfsc Scale length of disk arcsec e_Hfsc Formal fit error in Hfsc arcsec Hfes Central! (not effective) surface brightness of bulge mag/arcsec+2 e_Hfes Formal fit error in Hfes mag/arcsec+2 Hfer Bulge scale length (not effective radius) arcsec e_Hfer Formal fit error in Hfer arcsec Hfbc Central brightness of the bar arcsec e_Hfbc Formal fit error in Hfbc arcsec Hfma Bar major axis arcsec e_Hfma Formal fit error in Hfma arcsec Hfmi Bar minor axis arcsec e_Hfmi Formal fit error in Hfmi arcsec Hfpa Position angle of the bar deg e_Hfpa Formal fit error in Hfpa deg Kfcs Central surface brightness of the disk mag/arcsec+2 e_Kfcs Formal fit error in Kfcs (real uncertainty in general much larger) mag/arcsec+2 Kfsc Scale length of disk arcsec e_Kfsc Formal fit error in Kfsc arcsec Kfes Central! (not effective) surface brightness of bulge mag/arcsec+2 e_Kfes Formal fit error in Kfes mag/arcsec+2 Kfer Bulge scale length (not effective radius) arcsec e_Kfer Formal fit error in Kfer arcsec Kfbc Central brightness of the bar mag/arcsec+2 e_Kfbc Formal fit error in Kfbc mag/arcsec+2 Kfma Bar major axis arcsec e_Kfma Formal fit error in Kfma arcsec Kfmi Bar minor axis arcsec e_Kfmi Formal fit error in Kfmi arcsec Kfpa Position angle of the bar deg e_Kfpa Formal fit error in Kfpa deg Decompositions using the 1D technique with R^(1/4) law bulge UGC Name of galaxy in UGC <VII/26> --- Bfcs Central surface brightness of the disk mag/arcsec+2 e_Bfcs Fit error due to sky uncertainties in Bfcs mag/arcsec+2 Bfsc Scale length of disk arcsec e_Bfsc Fit error due to sky uncertainties in Bfsc arcsec Bfes Effective surface brightness of bulge mag/arcsec+2 e_Bfes Fit error due to sky uncertainties in Bfes mag/arcsec+2 Bfer Effective radius of the bulge arcsec e_Bfer Fit error due to sky uncertainties in Bfer arcsec Vfcs Central surface brightness of the disk mag/arcsec+2 e_Vfcs Fit error due to sky uncertainties in Vfcs mag/arcsec+2 Vfsc Scale length of disk arcsec e_Vfsc Fit error due to sky uncertainties in Vfsc arcsec Vfes Effective surface brightness of bulge mag/arcsec+2 e_Vfes Fit error due to sky uncertainties in Vfes mag/arcsec+2 Vfer Effective radius of the bulge arcsec e_Vfer Fit error due to sky uncertainties in Vfer arcsec Rfcs Central surface brightness of the disk mag/arcsec+2 e_Rfcs Fit error due to sky uncertainties in Rfcs mag/arcsec+2 Rfsc Scale length of disk arcsec e_Rfsc Fit error due to sky uncertainties in Rfsc arcsec Rfes Effective surface brightness of bulge mag/arcsec+2 e_Rfes Fit error due to sky uncertainties in Rfes mag/arcsec+2 Rfer Effective radius of the bulge arcsec e_Rfer Fit error due to sky uncertainties in Rfer arcsec Ifcs Central surface brightness of the disk mag/arcsec+2 e_Ifcs Fit error due to sky uncertainties in Ifcs mag/arcsec+2 Ifsc Scale length of disk arcsec e_Ifsc Fit error due to sky uncertainties in Ifsc arcsec Ifes Effective surface brightness of bulge mag/arcsec+2 e_Ifes Fit error due to sky uncertainties in Ifes mag/arcsec+2 Ifer Effective radius of the bulge arcsec e_Ifer Fit error due to sky uncertainties in Ifer arcsec Hfcs Central surface brightness of the disk mag/arcsec+2 e_Hfcs Fit error due to sky uncertainties in Hfcs mag/arcsec+2 Hfsc Scale length of disk arcsec e_Hfsc Fit error due to sky uncertainties in Hfsc arcsec Hfes Effective surface brightness of bulge mag/arcsec+2 e_Hfes Fit error due to sky uncertainties in Hfes mag/arcsec+2 Hfer Effective radius of the bulge arcsec e_Hfer Fit error due to sky uncertainties in Hfer arcsec Kfcs Central surface brightness of the disk mag/arcsec+2 e_Kfcs Fit error due to sky uncertainties in Kfcs mag/arcsec+2 Kfsc Scale length of disk arcsec e_Kfsc Fit error due to sky uncertainties in Kfsc arcsec Kfes Effective surface brightness of bulge mag/arcsec+2 e_Kfes Fit error due to sky uncertainties in Kfes mag/arcsec+2 Kfer Effective radius of the bulge arcsec e_Kfer Fit error due to sky uncertainties in Kfer arcsec Decompositions using the 1D technique with R^(1/2) law bulge Decompositions using the 1D technique with an exponential bulge UGC Name of galaxy in UGC <VII/26> --- Bfcs Central surface brightness of the disk mag/arcsec+2 e_Bfcs Fit error due to sky uncertainties in Bfcs mag/arcsec+2 Bfsc Scale length of disk arcsec e_Bfsc Fit error due to sky uncertainties in Bfsc arcsec Bfes Central! (not effective) surface brightness of bulge number=1 tableff: add 2.5*lg(39.3305) to get effective surface brightness tableef: add 2.5*lg(5.36019) to get effective surface brightness mag/arcsec+2 e_Bfes Fit error due to sky uncertainties in Bfes mag/arcsec+2 Bfer Bulge scale length (not eff. radius) number=2 tableef: multiply by 1.679 to get effective radius arcsec e_Bfer Fit error due to sky uncertainties in Bfer arcsec Vfcs Central surface brightness of the disk mag/arcsec+2 e_Vfcs Fit error due to sky uncertainties in Vfcs mag/arcsec+2 Vfsc Scale length of disk arcsec e_Vfsc Fit error due to sky uncertainties in Vfsc arcsec Vfes Central! (not effective) surface brightness of bulge number=1 tableff: add 2.5*lg(39.3305) to get effective surface brightness tableef: add 2.5*lg(5.36019) to get effective surface brightness mag/arcsec+2 e_Vfes Fit error due to sky uncertainties in Vfes mag/arcsec+2 Vfer Bulge scale length (not eff. radius) number=2 tableef: multiply by 1.679 to get effective radius arcsec e_Vfer Fit error due to sky uncertainties in Vfer arcsec Rfcs Central surface brightness of the disk mag/arcsec+2 e_Rfcs Fit error due to sky uncertainties in Rfcs mag/arcsec+2 Rfsc Scale length of disk arcsec e_Rfsc Fit error due to sky uncertainties in Rfsc arcsec Rfes Central! (not effective) surface brightness of bulge number=1 tableff: add 2.5*lg(39.3305) to get effective surface brightness tableef: add 2.5*lg(5.36019) to get effective surface brightness mag/arcsec+2 e_Rfes Fit error due to sky uncertainties in Rfes mag/arcsec+2 Rfer Bulge scale length (not eff. radius) number=2 tableef: multiply by 1.679 to get effective radius arcsec e_Rfer Fit error due to sky uncertainties in Rfer arcsec Ifcs Central surface brightness of the disk mag/arcsec+2 e_Ifcs Fit error due to sky uncertainties in Ifcs mag/arcsec+2 Ifsc Scale length of disk arcsec e_Ifsc Fit error due to sky uncertainties in Ifsc arcsec Ifes Central! (not effective) surface brightness of bulge number=1 tableff: add 2.5*lg(39.3305) to get effective surface brightness tableef: add 2.5*lg(5.36019) to get effective surface brightness mag/arcsec+2 e_Ifes Fit error due to sky uncertainties in Ifes mag/arcsec+2 Ifer Bulge scale length (not eff. radius) number=2 tableef: multiply by 1.679 to get effective radius arcsec e_Ifer Fit error due to sky uncertainties in Ifer arcsec Hfcs Central surface brightness of the disk mag/arcsec+2 e_Hfcs Fit error due to sky uncertainties in Hfcs mag/arcsec+2 Hfsc Scale length of disk arcsec e_Hfsc Fit error due to sky uncertainties in Hfsc arcsec Hfes Central! (not effective) surface brightness of bulge number=1 tableff: add 2.5*lg(39.3305) to get effective surface brightness tableef: add 2.5*lg(5.36019) to get effective surface brightness mag/arcsec+2 e_Hfes Fit error due to sky uncertainties in Hfes mag/arcsec+2 Hfer Bulge scale length (not eff. radius) number=2 tableef: multiply by 1.679 to get effective radius arcsec e_Hfer Fit error due to sky uncertainties in Hfer arcsec Kfcs Central surface brightness of the disk mag/arcsec+2 e_Kfcs Fit error due to sky uncertainties in Kfcs mag/arcsec+2 Kfsc Scale length of disk arcsec e_Kfsc Fit error due to sky uncertainties in Kfsc arcsec Kfes Central! (not effective) surface brightness of bulge number=1 tableff: add 2.5*lg(39.3305) to get effective surface brightness tableef: add 2.5*lg(5.36019) to get effective surface brightness mag/arcsec+2 e_Kfes Fit error due to sky uncertainties in Kfes mag/arcsec+2 Kfer Bulge scale length (not eff. radius) number=2 tableef: multiply by 1.679 to get effective radius arcsec e_Kfer Fit error due to sky uncertainties in Kfer arcsec Patricia Bauer CDS 1996 Jun 18 Roelof de Jong <R.S.deJong@durham.ac.uk> J_A+AS_118_557.xml Galaxy populations in the distant galaxy clusters. I. Cl0939+472 (z=0.41) and Cl0016+161 (z=0.54). I. J/A+AS/118/65 J/A+AS/118/65 BRI & redshifts in Cl0939+472 & Cl0016+161 Galaxy populations in the distant galaxy clusters. I. Cl0939+472 (z=0.41) and Cl0016+161 (z=0.54). I. P Belloni H -J Roeser Astron. Astrophys. Suppl. Ser. 118 65 1996 1996A&AS..118...65B Clusters, galaxy Redshifts galaxies: clusters: general galaxies: clusters: individual (Cl 0939+479, CI 0016+161) galaxies: distances and redshifts galaxies: evolution We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.
Cl 0939+479 ACO 851 09 42.8 +47 00 Cl 0016+161 00 18.5 +16 26
Data of 323 objects with R>22.5mag in Cl 10939+47 field Data of 200 objects with R>22.5mag in Cl 10016+161 field No Sequence number --- Xpos X coordinate arcsec Ypos Y coordinate arcsec Rmag R magnitude mag B-R B-R color mag n_B-R Note no B-R number=1 An '?' indicates objects that could not be fitted by any of the templates at any redshift between z=0.3 and z=0.7 --- B-I B-I color mag n_B-I Note no B-I number=1 An '?' indicates objects that could not be fitted by any of the templates at any redshift between z=0.3 and z=0.7 --- D4000 4000A-break index --- zD92 Redshitf from Dressler & Gunn, 1992 --- z Redshift --- n_z Note on z, s = star number=1 An '?' indicates objects that could not be fitted by any of the templates at any redshift between z=0.3 and z=0.7 --- e_z rms uncertainty on z --- n_e_z Note on e_z number=1 An '?' indicates objects that could not be fitted by any of the templates at any redshift between z=0.3 and z=0.7 --- MType Morphological type --- Patricia Bauer CDS 1996 Apr 12 Paola Belloni <belloni@usm.uni-muenchen.de> J_A+AS_118_65.xml Photometric and morphological analysis of UCM galaxies. I. Observations and reductions. Morphological classifications J/A+AS/118/7 J/A+AS/118/7 Photometry & morphology of UCM galaxies Photometric and morphological analysis of UCM galaxies. I. Observations and reductions. Morphological classifications A G Vitores J Zamorano M Rego O Alonso J Gallego Astron. Astrophys. Suppl. Ser. 118 7 1996 1996A&AS..118....7V Galaxy catalogs Morphology Photometry, surface Redshifts atlases galaxies: fundamental parameters galaxies: general galaxies: photometry surveys We present the results of Thuan & Gunn r CCD imaging observations of the Universidad Complutense de Madrid (UCM) sample of emission-line galaxies (ELGs), selected by the presence of H{alpha} emission in low-resolution objective prism spectra. In this work we characterize photometrically and morphologically a total of 212 objects from the UCM survey. This Paper presents the observations and basic reductions, and lists a set of photometric parameters calculated for each UCM object. In addition, for the first time in a ELGs sample, we have determined the morphological classification of the objects using simultaneously five different criteria.
Apparent and absolute magnitudes of UCM objects Name UCM name --- rmag Apparent magnitude in the Thuan-Gunn r band mag e_rmag rms uncertainty on r apparent magnitude mag z Redshift --- Dist Distance Mpc GalExt Galactic extinction mag rmagAbs Absolute magnitude in the Thuan-Gunn r band mag e_rmagAbs rms uncertainty on r absolute magnitude mag B+D decomposition parameters for UCM objects Name UCM name --- SuBrB Effective bulge surface brightness mag/arcsec2 e_SuBrB rms uncertainty on SuBrB mag/arcsec2 radB Effective radius of the bulge component arcsec e_radB rms uncertainty on radB arcsec Eps Ellipticity --- SuBrD Disk face-on extrapolated central surface brightness mag/arcsec2 e_SuBrD rms uncertainty on SuBrD mag/arcsec2 Length Scale length of the disk arcsec e_Length rms uncertainty on Length arcsec B/D Bulge-to-disk ratio --- e_B/D rms uncertainty on B/D --- rms rms scatter of the global B+D fit --- Photometric parameters of UCM objects Name UCM name --- a Major axis at 24 mag/arcsec2 isophote arcsec b Minor axis at 24 mag/arcsec2 isophote arcsec Rad1 Equivalent radius at 24 mag/arcsec2 isophote arcsec mag1 Apparent magnitude inside 24 mag/arcsec2 isophote mag Rad2 Equivalent radius at 24.5 mag/arcsec2 isophote arcsec mag2 Apparent magnit. inside 24.5 mag/arcsec2 isophote mag Mean photometric parameters and concentration indices of UCM objects. Name UCM name --- Rad Effective radius arcsec SuBr Mean surface brightness inside effective radius mag/arcsec2 SuBr2 Mean surface brightness inside 24.5 isophote mag/arcsec2 c31 Concentration index c31 number=1 C31 was introduced by deVaucoleurs (1977, 'Evolution of Galaxies and Stellar Populations' ed. Larson, R. & Tinsley, B., Yale University Observatory, New Haven, 43) and is the ratio of the radii which contain 75% and 25% of the total luminosity of the galaxy respectively (C31=r75/r25) --- c42 Concentration index c42 number=2 C42 was introduced by Kent (1985, ApJS 59,115) and is obtained with the ratio of the radii which contain 80% and 20% of the total luminosity of the galaxy (C42=5log(r80/r20)) --- cin Concentration index cin (alpha = 0.3) --- Morphological type, according to the different photometric criteria, for objects of UCM sample Name UCM name --- Mtype1 Morphological classif. according to B/D --- Mtype2 Morphological classif. according to cin (alpha) vs mean surface brightness inside 24.5 isophote --- Mtype3 Morphological classif. according to c31 --- Mtype4 Morphological classif. according to c42 --- Mtype5 Morphological classif. according to mean surface effective brightness --- Mtype Final Type --- Special comments on individual UCM objects Name UCM name --- Com Comments (several lines per galaxy) --- Patricia Bauer CDS 1995 Nov 27 <jaz@ucmast.fis.ucm.es> J_A+AS_118_7.xml Fractional abundances of molecules in dense interstellar clouds: a compendium of recent model results J/A+AS/119/111 J/A+AS/119/111 Molecular abundances in dense interstellar clouds Fractional abundances of molecules in dense interstellar clouds: a compendium of recent model results H -H Lee R P A Bettens E Herbst Astron. Astrophys. Suppl. Ser. 119 111 1996 1996A&AS..119..111L Abundances Interstellar medium ISM: abundances ISM: clouds ISM: molecules molecular processes In this paper we present calculated fractional abundances in dense interstellar clouds for selected atomic and molecular species using three different homogeneous, pseudo-time-dependent models discussed by Bettens, Lee, & Herbst (1995): the new standard model, the new neutral-neutral model, and model 4. We have run each model with 3 different hydrogen densities - 1,000; 10,000; and 100,000cm-3 - and two temperatures - 10K and 50K. "Low metal" elemental abundances have been used for all three models; the new standard model has also been run with "high metal" abundances.
New standard model: n=10+3 cm-3,T=10K New standard model: n=10+3 cm-3,T=50K New standard model: n=10+4 cm-3,T=10K New standard model: n=10+4 cm-3,T=50K New standard model: n=10+5 cm-3,T=10K New standard model: n=10+5 cm-3,T=50K New neutral-neutral model: n=10+3 cm-3,T=10K New neutral-neutral model: n=10+3 cm-3,T=50K New neutral-neutral model: n=10+4 cm-3,T=10K New neutral-neutral model: n=10+4 cm-3,T=50K New neutral-neutral model: n=10+5 cm-3,T=10K New neutral-neutral model: n=10+5 cm-3,T=50K Model 4: n=10+3 cm-3,T=10K Model 4: n=10+3 cm-3,T=50K Model 4: n=10+4 cm-3,T=10K Model 4: n=10+4 cm-3,T=50K Model 4: n=10+5 cm-3,T=10K Model 4: n=10+5 cm-3,T=50K New standard model(high metal): n=10+3 cm-3,T=10K New standard model(high metal): n=10+3 cm-3,T=50K New standard model(high metal): n=10+4 cm-3,T=10K New standard model(high metal): n=10+4 cm-3,T=50K New standard model(high metal): n=10+5 cm-3,T=10K New standard model(high metal): n=10+5 cm-3,T=50K Species Species name --- A4.5 Fractional abundances at 10+4.5 years cm-3 A5 Fractional abundances at 10+5 years cm-3 A5.5 Fractional abundances at 10+5.5 years cm-3 Ass Fractional abundances at steady state cm-3 table2.tex plain LaTeX version of table2a and table2b table3.tex plain LaTeX version of table3a and table3b table4.tex plain LaTeX version of table4a and table4b table5.tex plain LaTeX version of table5a and table5b table6.tex plain LaTeX version of table6a and table6b table7.tex plain LaTeX version of table7a and table7b table8.tex plain LaTeX version of table8a and table8b table9.tex plain LaTeX version of table9a and table9b table10.tex plain LaTeX version of table10a and table10b table11.tex plain LaTeX version of table11a and table11b table12.tex plain LaTeX version of table12a and table12b table13.tex plain LaTeX version of table13a and table13b UNKNOWN 1996 Feb 15 H.H. Lee <hhlee@pacific.mps.ohio-state.edu> J_A+AS_119_111.xml Sky brightness at the ESO La Silla Observatory 1978 to 1988. J/A+AS/119/153 J/A+AS/119/153 La Silla Observatory sky brightness 1978-1988 Sky brightness at the ESO La Silla Observatory 1978 to 1988. K Mattila P Vaisaenen G F O V Appen-Schnur Astron. Astrophys. Suppl. Ser. 119 153 1996 1996A&AS..119..153M J/A+AS/112/99 : Calar Alto Observatory sky brightness measurements Earth atmospheric effects interplanetary medium site testing techniques: photometric We have measured the sky brightness at the European Southern Observatory (ESO), La Silla, during 40 moonless nights in the years 1978-1988. Most of the measurements were performed in five intermediate band filters between 3500 and 5470A, including the Stroemgren u, b, and y bands. In addition we made measurements in the uvgr and BVRI photometric systems. Typically 20 to 40 readings were obtained each night at a fixed ({alpha}, {delta}) position, selected to be free of stars down to a limiting magnitude of B=~20. The sky brightnesses were calibrated using standard stars. We discuss the sky brightness variations both during individual nights and from year to year. We have found that the long-term variations are well correlated with the solar activity, for which the 10.7cm radio flux is used as a measure. We compare the sky brightnesses as observed at La Silla with the published values for several other sites. Finally, based on the tight correlation of the airglow variations in two pass bands near 4000A we propose a new method for the separation of airglow and zodiacal light contributions.
fig3a1.ps Intermediate-band filters night sky brightness fig3a2.ps Intermediate-band filters night sky brightness fig3a3.ps Intermediate-band filters night sky brightness fig3a4.ps Intermediate-band filters night sky brightness fig3a5.ps Intermediate-band filters night sky brightness fig3a6.ps Intermediate-band filters night sky brightness fig3a7.ps Intermediate-band filters night sky brightness fig3a8.ps Intermediate-band filters night sky brightness fig3a9.ps Intermediate-band filters night sky brightness fig3a10.ps Intermediate-band filters night sky brightness fig3a11.ps Intermediate-band filters night sky brightness fig3a12.ps Intermediate-band filters night sky brightness fig3a13.ps Intermediate-band filters night sky brightness fig3a14.ps Intermediate-band filters night sky brightness fig3a15.ps Intermediate-band filters night sky brightness fig3a16.ps Intermediate-band filters night sky brightness fig3a17.ps Intermediate-band filters night sky brightness fig3a18.ps Intermediate-band filters night sky brightness fig3a19.ps Intermediate-band filters night sky brightness fig3a20.ps Intermediate-band filters night sky brightness fig3a21.ps Intermediate-band filters night sky brightness fig3a22.ps Intermediate-band filters night sky brightness fig3a23.ps Intermediate-band filters night sky brightness fig3a24.ps Intermediate-band filters night sky brightness fig3b1.ps BVRI filters night sky brightness fig3b2.ps BVRI filters night sky brightness fig3b3.ps BVRI filters night sky brightness fig3b4.ps BVRI filters night sky brightness fig3b5.ps BVRI filters night sky brightness fig3b6.ps BVRI filters night sky brightness fig3b7.ps BVRI filters night sky brightness fig3b8.ps BVRI filters night sky brightness fig3c1.ps uvgr filters night sky brightness fig3c2.ps uvgr filters night sky brightness fig3c3.ps uvgr filters night sky brightness fig3c4.ps uvgr filters night sky brightness fig3c5.ps uvgr filters night sky brightness fig3c6.ps uvgr filters night sky brightness fig41-3.ps Correlations between intensities of different bands with the y band fig44-7.ps Correlations between intensities of different bands with the y band fig48-11.ps Correlations between intensities of different bands with the y band Patricia Bauer CDS 1996 Mar 25 Petri Vaisanen <pvaisane@mars.harvard.edu> J_A+AS_119_153.xml The peculiar B[e] star HD 45677. I. Photometric observations. J/A+AS/119/1 J/A+AS/119/1 HD 45677 photometry The peculiar B[e] star HD 45677. I. Photometric observations. D De Winter M E van den Ancker M R Perez J -P Swings P S The S B Johnson F J Molster J T van Loon Astron. Astrophys. Suppl. Ser. 119 1 1996 1996A&AS..119....1D Photometry Stars, emission circumstellar matter infrared: stars stars: emission-line, Be stars: individual (HD 45677) This short paper presents previously unpublished, as well as new, photometric observations of the peculiar B[e] star HD 45677. The photometric measurements were made in the Walraven WULBV, Stroemgren uvby, Johnson/Cousins UBV(RI)_C_ and the ESO JHKLM photometric systems between 1977 and 1994. Together with all the previously published photometry, these data will be analyzed in a separate paper, which will also investigate the spectroscopic behaviour of this fascinating object. For a description of the Walraven, Stroemgreen and JHKLM photometric systems, see e.g., <GCPD/11>, <GCPD/04> and <GCPD/09>.
HD 45677 06 28 17.4 -13 03 10
Walraven photometric data HJD Heliocentric julian date d Vint Visual intensity V mag B-V Walraven B-V color index mag B-L Walraven B-L color index mag B-U Walraven B-U color index mag B-W Walraven B-W color index mag Vmag Johnson V magnitude mag Unpublished and new Stroemgren photometric data HJD Heliocentric Julian Date d ymag Stromgren magnitude y mag b-y Stromgren colour b-y mag m1 Stromgren colour index m1 mag c1 Stromgren colour index c1 mag beta Stromgren beta index mag Unpublished and new UBV(RI)_C observations HJD Heliocentric Julian Date d Vmag Visual magnitude V mag U-B Johnson colour U-B mag B-V Johnson colour B-V mag V-R Cousins colour V-R mag V-I Cousins colour V-I mag Unpublished JHKLM photometry HJD Heliocentric Julian Date d Jmag Magnitude J mag Hmag Magnitude H mag Kmag Magnitude K mag Lmag Magnitude L mag Mmag Magnitude M mag table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 table4.tex LaTeX version of table4 Patricia Bauer CDS 1996 Mar 15 Dolf de Winter, jr., <DOLF@astro.uva.nl> J_A+AS_119_1.xml Deep CCD photometry and the initial mass function of the core of the OB cluster Berkeley 86. J/A+AS/119/221 J/A+AS/119/221 UBVRI photometry of stars in Berkeley 86 Deep CCD photometry and the initial mass function of the core of the OB cluster Berkeley 86. H J Deeg Z Ninkov Astron. Astrophys. Suppl. Ser. 119 221 1996 1996A&AS..119..221D Clusters, open Photometry, CCD open clusters and associations: individual (Bky 86) stars: luminosity function, mass function Based on photometry of deep CCD frames of the central region of the OB cluster Berkeley 86, we derive the cluster mass function. The absence of current star formation, and the cluster's young age of about 6Myrs, leads to the conclusion that the initial mass function (IMF) and the current mass function are identical for stars with m<10m_{sun}_. In the range of 1.2-20m_{sun}_, an IMF with a slope of {GAMMA}=-1.3+/-0.3 is found. This value agrees well with other recent determinations of young clusters IMFs which are close to the classical Salpeter IMF with {GAMMA}=-1.35. Sections of the IMF of Berkeley 86 that are significantly steeper, or flatter, are most likely the result of a dip in the star's mass distribution in the range of 3.5-10m_{sun}_. Similar dips may have led to steep IMFs over narrow mass ranges, as reported in the literature for some other clusters. No sign for a low mass turn-over in the IMF of Berkeley 86 is found for masses extending down to 0.85 m_{sun}_.
UBVRI photometry of 544 stars in Bky86 ID ID number of stars in this paper --- Forbes-ID ID number of stars in Forbes et al. (1992AJ....103..916F) number=1 ID 162 = Forbes-ID 1 is also HD228969 --- RAdeg Right Ascencion (J2000) number=2 Precision is about 1 arcsec. deg DEdeg Declination (J2000) number=2 Precision is about 1 arcsec. deg Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag U-B U-B color index mag e_U-B rms uncertainty on U-B mag B-V B-V color index mag e_B-V rms uncertainty on B-V mag V-R V-R color index mag e_V-R rms uncertainty on V-R mag R-I R-I color index mag e_R-I rms uncertainty on R-I mag E(B-V) E(B-V) extinction mag logM log mass of cluster-members; 9.99= non-member; only entries for stars with V<18.5 solMass Patricia Bauer CDS 1996 Apr 25 Hans-Jorg Deeg <hdeeg@ll.iac.es> J_A+AS_119_221.xml A large sample of objective prism quasar candidate. J/A+AS/119/265 J/A+AS/119/265 High probability quasar candidates A large sample of objective prism quasar candidate. A Iovino R Clowes P Shaver Astron. Astrophys. Suppl. Ser. 119 265 1996 1996A&AS..119..265I QSOs quasars: general surveys The Automated Quasar Detection (AQD) technique has been applied to six connected fields near the South Galactic Pole. A comparison with the Veron & Veron catalogue (1993) <VII/188> and the Cristiani et al. compilation (1995A&AS..112..347C) shows that AQD rediscovered ~75% of the known quasars with non-overlapping objective-prism spectra present in these fields (~40% if considering only the high degree candidates). A list of 1592 high grade candidates is given, including the results of cross-correlation with X-ray and radio catalogues.
List of high probability candidates RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec mcosmos Prism instrumental magnitude mag Vcosmos Indicative magnitude in the V band mag zlya Tentative redshift --- GRADE Grade --- Notes Notes number=1 ? - possible overlapping spectrum * - good quality candidate Q - known quasar X - known ROSAT X--ray source R - known radio source --- Patricia Bauer CDS 1996 Mar 25 A. Iovino <iovino@brera.mi.astro.it> J_A+AS_119_265.xml Be stars in open clusters. I. uvby{beta} photometry. J/A+AS/119/271 J/A+AS/119/271 Be stars uvby{beta} photometry Be stars in open clusters. I. uvby{beta} photometry. J Fabregat J M Torrejon P Reig G Bernabeu J Busquets A Marco V Reglero Astron. Astrophys. Suppl. Ser. 119 271 1996 1996A&AS..119..271F Photometry Stars, emission open clusters and associations: general stars: emission-line, Be techniques: photometric We present uvby{beta} photometry for Be stars in eight open clusters and two OB associations. It is shown that Be stars occupy anomalous positions in the photometric diagrams, which can be explained in terms of the circumstellar continuum radiation contribution to the photometric indices. In the (b-y)_0_-M_V_ plane Be stars appear redder than the non emission B stars, due to the additional reddening caused by the hydrogen free-bound and free-free recombination in the circumstellar envelope. In the c_0_-M_V_ plane the earlier Be stars present lower c_0_ values than absorption-line B stars, which is caused by emission in the Balmer discontinuity, while the later Be stars deviate towards higher c_0_ values, indicating absorption in the Balmer discontinuity of circumstellar origin.
Catalogue of 22 observed stars Name Star name --- Vmag V magnitude mag b-y b-y color index mag m1 m1 color index mag c1 c1 color index mag Hbeta Hbeta color index mag N Number of measures --- e_Vmag rms uncertainty on Vmag mag e_b-y rms uncertainty on b-y mag e_m1 rms uncertainty on m1 mag e_c1 rms uncertainty on c1 mag e_Hbeta rms uncertainty on Hbeta mag DVmag Standard value minus transformed value mag Db-y Standard value minus transformed value mag Dm1 Standard value minus transformed value mag Dc1 Standard value minus transformed value mag DHbeta standard value minus transformed value mag Photometric data for Be stars Photometric data for B stars not classified as Be Cluster Open cluster or association name --- No Star number number=1 the following designations were taken: h and chi Per: star number from Oosterhoff (1937AnLei..17a...1O) NGC 663: star number from Wallenquist (1929MeUpp..42.....W) Pleiades: star number from Hertzsprung (1947AnLei..19....3H) alpha Per: star number from Heckmann et al. (1956AN....283..109H) Orion OB1: star number from Warren and Hesser (1977ApJS...34..115W) NGC 2323: star number from Cuffey (1941ApJ....94...55C) NGC 2422: star number from Schewick (1966VeBon..74....1V) NGC 6611: star number from Walker (1961ApJ...133..438W) NGC 7654: star number from Lundby (1946UppAn...1j...1L) Cepheus OB3: star number from Blaauw et al. (1959ApJ...130...69) --- Name HD or BD designation --- n_Name Note on name (table13) --- Vmag V magnitude mag b-y b-y color index mag m1 m1 color index mag c1 c1 color index mag Hbeta Hbeta color index mag e_Vmag rms uncertainty on Vmag mag e_b-y rms uncertainty on b-y mag e_m1 rms uncertainty on m1 mag e_c1 rms uncertainty on c1 mag e_Hbeta rms uncertainty on Hbeta mag N Number of individual measurements --- Ref References (only for tab5-14) number=2 the numbers refer to the following references: 1.- Wackerling (1970MmRAS..73..153W) 2.- Hardorp et al., (1965), Catalogue <III/76> 3.- Slettebak (1968ApJ...154..933S) 4.- Fabregat et al., (1994, Be Star News. 29, 8) 5.- Schild & Romanishin (1976ApJ...204..493S) 6.- Gonzalez & Gonzalez (1954BOTT....1i...3G) 7.- Slettebak (1985ApJS...59..769S) 8.- Merrill & Burwell (1943ApJ....98..153M) 9.- Merrill & Burwell (1933ApJ....78...87M) 10.- Schild (1965ApJ...141..979S) 11.- Merrill & Burwell (1949ApJ...110..387M) 12.- Sanduleak & Bidelman (1980PASP...92...72S) 13.- Coyne et al. (1978VatOP...1..257C) 14.- Sanduleak (1990AJ....100.1239S) 15.- Dolidze (1975, Bull. Abastumani Astrophys. Obs. 47, 3) 16.- Bidelman (1976IAUS...70..457B) 17.- Irvine (1975ApJ...196..773I) 18.- Morgan et al. (1995ApJS....2...41M) 19.- Lesh (1968ApJS...17..371L) 20.- Bartkus (1964VilOB..13...29B) 21.- MacConnell (1961A&AS...44..387M) 22.- Dworetski (1976AJ.....80..131D) 23.- Walker (1961ApJ...133..438W) 24.- Hiltner (1956ApJS....2..389H) 25.- Bond (1973PASP...85..405B) 26.- Blaauw et al. (1959ApJ...130...69B) --- Note Notes number=3 The following symbols are used in the notes: *: Possible non-members (tab5-14) 1: Used as standard (table15) 2: Nonmember of the cluster or association (table15) 3: Chemically peculiar star (Ap or Am, Renson 1988A&AS...76..127R) (table15) 4: Variable star IL Cephei. Herbig Ae/Be star. (table15) --- table1.tex LaTeX version of table1 table5.tex LaTeX version of table5 table6.tex LaTeX version of table6 table7.tex LaTeX version of table7 table8.tex LaTeX version of table8 table9.tex LaTeX version of table9 table10.tex LaTeX version of table10 table11.tex LaTeX version of table11 table12.tex LaTeX version of table12 table13.tex LaTeX version of table13 table14.tex LaTeX version of table14 table15.tex LaTeX version of table15 Patricia Bauer CDS 1996 May 07 J_A+AS_119_271.xml Long-term monitoring of active stars. V. UBV(RI)c photometry collected in Feb-Mar 1990. J/A+AS/119/281 J/A+AS/119/281 UBV Long-term monitoring of active stars. V. UBV(RI)c photometry collected in Feb-Mar 1990. G Cutispoto Astron. Astrophys. Suppl. Ser. 119 281 1996 1996A&AS..119..281C J/A+AS/121/369 : UBVRI observations of active stars (Cutispoto, 1997) Photometry, Cousins Photometry, UBVRI Stars, variable stars: activity stars: late-type stars: variables: general High-precision UBV(RI)_c_ photometry of 12 selected active stars, collected at the European Southern Observatory (La Silla, Chile) over the period February-March 1990, is presented. Significant evolution of the light curves, period variations and, in most cases, evidence for long-term variability of the global degree of spottedness are found. Some of the spectral classifications are discussed. This paper is part of a more extensive program focusing on the global properties and evolution of active stars and is aimed at establishing a time-extended photometric database which can give important clues on topics such as the stability of the spotted areas, differential rotation and solar-like cycles. For a description of the UBV and (RI)c photometric systems, see e.g. General Catalog of Photometric Data <GCPD/01> and <GCPD/54>.
UBVRI photometry HD HD number --- Name Other name --- Date Observation period --- HJD Heliocentric Julian day d Phase Corresponding phase number=1 The phases are computed by using the following ephemeris: HD 26354 = AG Dor, HJD = 2447587.52 + 2.533 x E HD 45088 = OU Gem, HJD = 2443846.2 + 7.36 x E HD 82558 = LQ Hya, HJD = 2445275.993 + 1.6092 x E HD 98712 = SZ Crt, HJD = 2441389.0 + 11.58 x E HD 101309 = V829 Cen, HJD = 2447570.53 + 11.65 x E HD 102077 = V838 Cen, HJD = 2445805.4 + 1.88 x E HD 106225 = HU Vir, HJD = 2445214.7 + 10.50 x E HD 119285 = V851 Cen, HJD = 2447949.5 + 11.50 x E HD 127535 = V841 Cen, HJD = 2445804.1 + 5.929 x E HD 136905 = GX Lib, HJD = 2445061.901 + 11.13448 x E HD 139084 = V343 Nor, HJD = 2445801.9 + 4.25 x E HD 155555 = V824 Ara, HJD = 2445803.07 + 1.681652 x E --- Vmag V magnitude mag U-B U-B color index mag B-V B-V color index mag V-Rc V-R_c_ color index mag V-Ic V-I_c_ color index mag Patricia Bauer CDS 1996 Apr 26 G. Cutispoto <ESO@alpha.ct.astro.it> J_A+AS_119_281.xml M15, an astrometric standard for CDD observations. J/A+AS/119/307 J/A+AS/119/307 Position in M15 M15, an astrometric standard for CDD observations. J -F Le Campion J Colin M Geffert Astron. Astrophys. Suppl. Ser. 119 307 1996 1996A&AS..119..307L Clusters, globular Positional data astrometry globular clusters: individual (M 15) CCD observations of stars in the region of the globular cluster M15 have been used to obtain astrometric positions of 1092 stars in the central part of the cluster within the FK5 system. The purpose of this catalogue is to calibrate astrometrically CCD observations by means of measuring the positions of stars in M15. The comparison with other catalogues and with measurements of photographic plates of the central part of M15 indicates a mean accuracy of about 50 to 70mas for each star of our catalogue.
Astrometric positions of 1093 stars in the M15 central region of equinox J2000 No Identification number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec DRA Dispersion in right ascension arcsec DDE Dispersion in declination arcsec o_RA Number of measures retained in right ascension --- o_DE Number of measures retained in declination --- Patricia Bauer CDS 1996 Apr 06 Jean-Francois LE CAMPION <lecampion@observ.u-bordeaux.fr> J_A+AS_119_307.xml CCD sequences in the Shapley supercluster of galaxies. II. The ESO data. J/A+AS/119/329 J/A+AS/119/329 VR photometry in the Shapley Supercluster CCD sequences in the Shapley supercluster of galaxies. II. The ESO data. E Slezak L Infante H Quintana Astron. Astrophys. Suppl. Ser. 119 329 1996 1996A&AS..119..329S Clusters, galaxy Photometry galaxies: clusters: individual (Shapley supercluster) galaxies: photometry surveys techniques: photometric We present V and R CCD photometric sequences of stars and galaxies for calibrating ESO/SERC (R) survey plates in the region of the Shapley supercluster of galaxies.
*VR photometry ESO ESO field number --- Spot Spot designation --- No Rank number in the detection catalogue --- oRA Offset in right ascension from the centre of the frame arcsec oDE Offset in declination from the centre of the frame arcsec Vmag Magnitude in the V band mag e_Vmag Photometric error in the V band mag Rmag Magnitude in the R band mag e_Rmag Photometric error in the R band mag Patricia Bauer CDS 1996 May 02 Eric Slezak <slezak@purcell.obs-nice.fr> J_A+AS_119_329.xml A 330-360 GHz spectral survey of G 34.3+0.15. I. Data and physical analysis J/A+AS/119/333 J/A+AS/119/333 330-360GHz spectral lines of G 34.3+0.15. A 330-360 GHz spectral survey of G 34.3+0.15. I. Data and physical analysis G H Macdonald A G Gibb R J Habing T J Millar Astron. Astrophys. Suppl. Ser. 119 333 1996 1996A&AS..119..333M Interstellar medium ISM: abundances ISM: individual (G 34.3+0.15) ISM: molecules line: identification radio lines: ISM A 330-360 GHz spectral survey of the hot molecular core associated with the `cometary' ultracompact H II region G 34.3+0.15 observed with the James Clerk Maxwell Telescope has detected 338 spectral lines from at least 35 distinct chemical species. 70 lines remain unidentified. Chemical abundance and rotation temperature have been determined by rotation diagram analysis for 13 species, and lower limits to abundance found for 38 others. The spectral lines identified are tabulated in Table 1 in the form of observed frequency, line brightness temperature and width, the observing session in which the line was observed, the species, transition and its theoretical frequency (if a positive identification can be made). Any comments are listed in the final column.
Parameters of spectral lines detected nu_obs Observed frequency GHz TA Observed brightness temperature K u_TA Uncertainty flag number=1 The bracket indicates that the value listed is not likely to be accurate, most probably due to self-absorption and/or emission in the off-source reference beam --- Width Full-Width-at-Half-Maximum linewidth MHz u_Width Uncertainty flag number=1 The bracket indicates that the value listed is not likely to be accurate, most probably due to self-absorption and/or emission in the off-source reference beam --- code Observing run/observed sideband label number=2 The code indicates whether the line was detected in the first (1) or second (2) observing session, in the main (m) or image (i) band. --- species Molecular species name --- trans Transition --- nu_th Theoretical frequency GHz notes Notes number=3 * - If the identification of the species and transition is ambiguous, the various alternatives are given, with the favoured identification shown with an asterisk. ? - Question marks denote uncertain detections b - Blended lines are marked by `b'. --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 Apr 25 A.G.Gibb <agg@starlink.ukc.ac.uk> J_A+AS_119_333.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest. XIV: Be III and B III. J/A+AS/119/369 J/A+AS/119/369 Stark broadening. XIV: Be III and B III Stark broadening of spectral lines of multicharged ions of astrophysical interest. XIV: Be III and B III. M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 119 369 1996 1996A&AS..119..369D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles molecular data Using a semiclassical approach, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for 12 Be III and 27 B III multiplets. The obtained results have been compared with available experimental and theoretical data.
Stark broadening parameters due to e-, p- and He II-impacts for Be III and B III N Perturber density cm-3 El Element name --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for NV > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for NV > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe+ (4) --- WHe+ FWHM for He II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe+ (4) --- dHe+ shift for He II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1996 Apr 02 Milan S. Dimitrijevic <mdimitrijevic@aob.aob.bg.ac.yu> J_A+AS_119_369.xml Multi-colour photometric and spectroscopic monitoring of the WN5 star EZ Canis Majoris J/A+AS/119/37 J/A+AS/119/37 EZ CMa UBV & VBLUW photometry Multi-colour photometric and spectroscopic monitoring of the WN5 star EZ Canis Majoris M F J Duijsens K A van der Hucht A M van Genderen H E Schwarz H P J Linders O M Kolkman Astron. Astrophys. Suppl. Ser. 119 37 1996 1996A&AS..119...37D Photometry, UBV Photometry, Vilnius Stars, Wolf-Rayet binaries: close stars: individual (WR 6, HD 50896, EZ Cma) stars: variables: general stars: Wolf-Rayet We present and analyse photometric and spectroscopic observations of the WN5 star EZ Canis Majoris obtained over a period of 7 years. We discuss the changing light curve, the shift in phase of the maxima and point to flare type variability seen in one night. Small amplitude variations are reported in another night. We have investigated the change of the average visual magnitude over a time span of 18 years and found a tentative cyclic variation with a time scale of 2425d (6.6yr) with a range of ~0.07mag. This, of course, should be verified. If true, a precession phenomenon may offer an explanation. The trend of the maximum light amplitude of the 3.766d cycle is also investigated and it shows a saw-tooth character with a timescale of ~400d. A possible relation with the magnetic activity of the star is discussed. We conclude that the line emission variability can be caused by both a single star model with an ever-changing wind and a binary (WN+NS) model.
EZ CMa WR 6 HD 50896 06 54 12.97 -23 55 42.0
Relative Johnson magnitudes and colours of January 11 1987 through January 16 1987 HJD Heliocentric julian date d DVmag Relative V Johnson magnitude mag DB-V Relative Johnson B-V color mag DU-B Relative Johnson U-B color mag *Relative VBLUW data of EZ CMa, epoch I *Relative VBLUW data of EZ CMa, epoch II HJD Heliocentric julian date d DVmag Relative V magnitude (log intensity) mag DBmag Relative B magnitude (log intensity) mag DLmag Relative L magnitude (log intensity) mag DUmag Relative U magnitude (log intensity) mag DWmag Relative W magnitude (log intensity) mag Patricia Bauer CDS 1996 Feb 14 M.F.J. Duijsens <duijsens@strw.LeidenUniv.nl> J_A+AS_119_37.xml Photometry of seven clusters of galaxies at intermediate redshift (z=0.15-0.50) J/A+AS/119/391 J/A+AS/119/391 Gunn photometry of seven clusters of galaxies Photometry of seven clusters of galaxies at intermediate redshift (z=0.15-0.50) E Molinari A Buzzoni G Chincarini Astron. Astrophys. Suppl. Ser. 119 391 1996 1996A&AS..119..391M Clusters, galaxy Photometry galaxies: clusters: general galaxies: photometry Gunn g, r, i photometry for the 7 clusters MRC0254-274, Cl0317+15, MS0418.3-3 844, Cl1141-283, A1689, A3594, S0781B is presented. For each cluster we derived the spatial distribution properties obtaining the core radius and the concentration parameters. Color properties of the cluster galaxy population are also briefly discussed.
MRC 0254-274 02 56 51 -27 17 58 MS 0418.3-3844 1E 0418.3-3844 04 20 06 -38 37 34 ACO 1689 13 11.6 -01 22 ACO 3594 14 20.4 -17 45 Cl0317+15 03 20 03 +15 17 51 Cl1141-283 11 44 09 -28 35 08 ACO S 781 15 00 15 -18 08 19
Photometric catalog of cluster MRC0254-274 Photometric catalog of cluster Cl0317+15 Photometric catalog of cluster MS0418.3-3844 Photometric catalog of cluster Cl1141-283 Photometric catalog of cluster A1689 Photometric catalog of cluster A3594 Photometric catalog of cluster S0781B No ID number for object --- Xpos X coordinate from adopted center pix Ypos Y coordinate from adopted center pix gmag Gunn g isophotal magnitude mag rmag Gunn r isophotal magnitude mag imag Gunn i isophotal magnitude mag g-r g-r aperture color mag g-i g-i aperture color mag Rad Isophotal radius in r magnitude number=1 The pixel size is 0.675 arcsec for clusters Cl0317+15 Cl1141-283 A1689 A3594 S0781B 0.6075 arcsec for clusters MRC0254-274 MS0418.3-3844 pix Patricia Bauer CDS 1996 Apr 02 Emilio Molinari <molinari@merate.mi.astro.it> J_A+AS_119_391.xml NGC 2477: photometry and luminosity function. J/A+AS/119/413 J/A+AS/119/413 RI and Teff of stars in NGC 2477 NGC 2477: photometry and luminosity function. G Galaz M T Ruiz I Thompson M Roth Astron. Astrophys. Suppl. Ser. 119 413 1996 1996A&AS..119..413G Clusters, open Effective temperatures Photometry open clusters and associations: individual (NGC 2477) stars: luminosity function, mass function Trough photometric methods we have constructed the luminosity function for the southern open cluster NGC 2477 down to M_v_=~12. We present R-I color-magnitude diagrams and near-infrared color-color diagrams, which allow us to separate statistically the cluster stars from the field ones, numerous because of the galactic latitude of the cluster. Our luminosity function (LF) reproduces some features obtained by other authors, namely, a dip at M_v_=~7, and a probable maximum at M_v_=~12. The method developed to separate cluster stars from field stars could be of interest to other astronomical problems.
NGC 2477 07 52.3 -38 33
Reddest and faintest stars with a high probability to belong to the open cluster NGC 2477 No Star number. --- Xpos Horizontal position (or x position) in the plate 1 (x=0 is lower left corner) pix Ypos Vertical position (or y position) in the plate 1 (y=0 is lower left corner) pix Rmag Absolute magnitude in the R band Not corrected of extinction mag e_Rmag Photometric error of R magnitude mag Imag Absolute magnitude in the I band Not corrected of extinction mag e_Imag Photometric error of I magnitude mag Teff Effective temperature K e_Teff Error in the effective temperature K log(Teff) Base 10 logarithm of the effective temperature K e_log(Teff) Error in the logarithm of effective temperature K Patricia Bauer CDS 1996 Mar 28 Gaspar Galaz <galaz@iap.fr> J_A+AS_119_413.xml A search for OH maser emission from post-asymptotic giant branch stars. J/A+AS/119/459 J/A+AS/119/459 Search for OH maser emission A search for OH maser emission from post-asymptotic giant branch stars. P Te Lintel Hekkert J M Chapman Astron. Astrophys. Suppl. Ser. 119 459 1996 1996A&AS..119..459T J/A+A/297/494 : OH maser from semiregular variables J/A+A/277/453 : OH maser survey of cool IRAS sources Masers Stars, giant masers planetary nebulae: general radio lines: stars stars: AGB and post-AGB We present a survey for OH maser emission at 18cm in the direction of 196 IRAS point sources. The primary aim of the survey was to detect OH maser emission from post-asymptotic giant branch (post-AGB) stars. OH emission and/or absorption was detected in the direction of 77 sources of which 57 OH detections were previously unknown, giving an overall detection rate of 39 per cent. Fourteen maser sources associated with evolved stars or planetary nebulae were found, corresponding to 7 per cent of the total observed. These included three planetary nebulae (two new OH detections), nine post-AGB stars (three new OH detections) and two cold OH/IR stars (both previously known). Two sources were of uncertain identification (both new OH detections). The remainder of the OH sources were identified with young stellar objects and with HII regions. The survey included the detection of OH maser emission from HD 101584, an early-type supergiant at high Galactic latitude. For several of the post-AGB stars, changes have occurred in the OH spectral profiles over a period of several years. This is interpreted as evidence for rapid changes in the stellar winds, due either to interactions with stellar companions, novae-like events or rapid stellar evolution.
Results of the OH survey IRAS IRAS name --- Epoch Epoch of observations (mm/yy) --- F1612 Flux at 1612MHz number=1 The one-sigma rms values are given for the non-detections. Jy n_F1612 Note if non-detection number=2 E, A, E/A indicates that OH line emission (E) and/or absorption (A) was detected. A blank indicates that a transition was not observed. --- F1665 Flux at 1665MHz number=1 The one-sigma rms values are given for the non-detections. Jy n_F1665 Note if non-detection number=2 E, A, E/A indicates that OH line emission (E) and/or absorption (A) was detected. A blank indicates that a transition was not observed. --- F1667 Flux at 1667MHz number=1 The one-sigma rms values are given for the non-detections. Jy n_F1667 Note if non-detection number=2 E, A, E/A indicates that OH line emission (E) and/or absorption (A) was detected. A blank indicates that a transition was not observed. --- F1720 Flux at 1720MHz number=1 The one-sigma rms values are given for the non-detections. Jy n_F1720 Note if non-detection number=2 E, A, E/A indicates that OH line emission (E) and/or absorption (A) was detected. A blank indicates that a transition was not observed. --- Class Classification number=3 Classification of the source as described in the text. --- n_Class Note on classification number=4 ** indicates that it is a new OH detection --- Ref Literature reference number=5 References: 1. Beck et al. (1991ApJ...383..336B) 2. Brand et al. (1986A&AS...65..537B) 3. Braz & Epchtein (1983A&AS...54..167B) 4. Braz et al. (1989A&AS...77..465B) 5. Casali (1991MNRAS.248..229C) 6. Casoli et al. (1986A&A...169..281C) 7. Caswell & Haynes (1987AuJPh..40..215C) 8. Caswell et al. (1980AuJPh..33..639C) 9. Caswell & Haynes (1983AuJPh..36..361C) 10. Caswell & Haynes (1983AuJPh..36..417C) 11. Caswell et al. (1989AuJPh..42..331C) 12. Churchwell et al. (1990A&AS...83..119C) 13. Crawford & Rowan-Robinson (1986MNRAS.221..923C) 14. De Vries et al. (1984A&AS...56..333D) 15. Dong & Hu (1991AcApS..11..172D) 16. Fix & Mutel (1984AJ.....89..406F) 17. Gardner & Whiteoak (1984MNRAS.210...23G) 18. Gauvin & Strom (1992ApJ...385..217G) 19. Gaylar et al. (1994MNRAS.269..257G) 20. Graham & Hartigan (1988AJ.....95.1197G) 21. Haynes, Caswell & Goss (1976AuJPh...3...57H) 22. Henning et al. (1992A&AS...93..525H) 23. Hughes et al. (1991AJ....101.1013H) 24. Jenniskens & Wouterloot (1990A&A...227..553J) 25. Kastner et al. (1992ApJ...389..357K) 26. Lester et al. (1987ApJ...320..573L) 27. Loup et al. (1990A&A...227L..29L) 28. Macleod (1991MNRAS.252p..36M) 29. Macleod & Gaylard (1992MNRAS.256..519M) 30. Milman (1975ApJ...202..673M) 31. Moorwood & Salinari (1983A&A...125..342M ) 32. Norris et al. (1987ApJ...321..888N) 33. Nyman L.-A. et al. (1992A&AS...93..121N) 34. Odenwald (1989AJ.....97..801O) 35. Ogura & Walsh (1992ApJ...400..248O) 36. Payne, Philipps & Terzian (1988ApJ...326..368P) 37. Peng & Whiteoak (1992MNRAS.254..301P) 38. Persi et al. (1990AJ.....99..303P) 39. Persson & Campbell (1987AJ.....94..416P) 40. Persson & Campbell (1988AJ.....96.1019P) 41. Preite-Martinez (1988A&AS...76..317P) 42. Scalise et al. (1989A&A...221..105S) 43. Simpson & Rubin (1990ApJ...354..165S) 44. te Lintel Hekkert et al. (1988A&A...202L..19T) 45. te Lintel Hekkert et al. (1989A&AS...78..399T) 46. te Lintel Hekkert (1991A&AS...90..327T) 47. te Lintel Hekkert et al. (1992ApJ...390L..23T) 48. Van de Steene & Pottasch (<J/A+A/274/895>) 49. Weaver, Dieter & Williams (1968ApJS...16..219W) 50. Weintraub (1990ApJS...74..575W) 51. Woodward et al. (1985A&A...147...84W) 52. Zijlstra et al. (1989A&A...217..157Z) 53. This paper. --- table2.tex TeX version of table2 Patricia Bauer CDS 1996 May 24 Peter te Lintel Hekkert <plintel@atnf.CSIRO.AU> J_A+AS_119_459.xml UBV photometry of wide visual double stars. V. Double stars with mainly K- and M- type primaries. J/A+AS/119/483 J/A+AS/119/483 UBV photometry of double stars. UBV photometry of wide visual double stars. V. Double stars with mainly K- and M- type primaries. D Sinachopoulos E L van Dessel Astron. Astrophys. Suppl. Ser. 119 483 1996 1996A&AS..119..483S Photometry, UBV Stars, double and multiple binaries: visual We present UBV photometric observations of 55 wide visual double stars with K- and M- type primaries. Our observations have been compared and combined with information available in the literature. At least 58% of them are optical pairs.
UBV photometry of wide double stars with K- and M- type primaries IDS IDS code of the double star as listed in WDS (Worley and Douglass, 1984) --- Sep Angular separation arcsec SpA Spectral type of A component --- Vmag V magnitude of A component mag e_Vmag rms uncertainty on Vmag mag B-V B-V color index of A component mag e_B-V rms uncertainty on B-V mag U-B U-B color index of A component mag e_U-B rms uncertainty on U-B mag o_Vmag Number of observation for A component --- SpB Spectral type of B component --- Vmag2 V magnitude of B component mag e_Vmag2 rms uncertainty on Vmag2 mag B-V2 B-V color index of B component mag e_B-V2 rms uncertainty on B-V2 mag U-B2 U-B color index of B component mag e_U-B2 rms uncertainty on U-B2 mag o_Vmag2 Number of observation for B component --- The astrophysical data No Sequence number --- IDS IDS number --- m_IDS Component of the binary --- Sp Spectral type --- E(B-V) B-V extinction mag E(U-B) U-B extinction mag A(V) Visual absorption mag MV Absolute V magnitude mag Dist Distance pc Sep Separation AU Nat Nature number=1 PHY: physical pair PHY(?): probably a physical pair PHY?: either has CO components only, or they are in addition gravitationally bound CO?: two components of the system have common origin (born together, but not orbital motion) CO(?): either OPT or it has CO components OPT: optical pair --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 May 03 Dimitris Sinachopoulos <Dimitris.Sinachopoulos@oma.be> J_A+AS_119_483.xml Catalogue of solar type II radio bursts observed from September 1990 to December 1993 and their statistical analysis J/A+AS/119/489 J/A+AS/119/489 Solar Type II Radio Bursts, 1990.09 - 1993.12 Catalogue of solar type II radio bursts observed from September 1990 to December 1993 and their statistical analysis G Mann A Klassen H -T Classen H Aurass D Scholz R J MacDowall R G Stone Astron. Astrophys. Suppl. Ser. 119 489 1996 1996A&AS..119..489M Sun Sun: activity Sun: radio radiation Solar type II radio bursts represent the radio signature of shock waves travelling through the solar corona. They are associated with flares, coronal mass ejections (CME's) and interplanetary shocks. Type II radio bursts appear as emission stripes slowly drifting from high to low frequencies in dynamic radio spectra. The spectral features of all solar type II radio bursts observed by the new radiospectrograph of the Astrophysikalisches Institut Potsdam in Tremsdorf during the time period from September 1, 1990 to December 31, 1993, i.e., during the first part of the ULYSSES spacecraft mission, are summarized and statistically investigated.
Solar type II radio bursts (Sep 1990-Dec 1993) OBSdate Date of observation "DD/MM/YY" OBShs Start time of observation (hours) h OBSms Start time of observation (minutes) min n_OBSms Note on start time of observation number=1 E, early as given; U, later than given --- OBShe End time of observation (hours) h OBSme End time of observation (minutes) min n_OBSme Note on end time of observation number=1 E, early as given; U, later than given --- Even Kind of event number=2 I,II,III,IV,V: type I,II,III,IV,V burst UNCLF: unclassified events B: single burst S: storm bursts U: type U bursts G: small group of bursts (<10) GG: large group of bursts (>10) C: any continuum underlying other events F: fluctuating continuum RS: reverse drift bursts H: herringbones P: pulsations Z: zebra bursts HARM: harmonic emission SPIKES: spikes bursts DCIM: events in the decimetric range --- LowFreq Lower value of the frequence range MHz UppFreq Upper value of the frequence range MHz Observed solar type II radio bursts No Sequential number --- n_No a for average (last line) --- Date Observation date "DD/MM/YY" Day [1/365] Number of the day --- UTh Begining of observation time (UT hours) h UTm Begining of observation time (UT min) min UTh2 End of observation time (UT hours) h UTm2 End of observation time (UT min) min Struct General spectral structure (fundamental (F), harmonic (H)) --- <Deltaf/f> Mean value of the instantaneous bandwidth --- e_<Deltaf/f> rms uncertainty on Deltaf --- <Deltaf/f>F Fundamental band instantaneous bandwidth --- <Deltaf/f>H Harmonic band instantaneous bandwidth --- <Df> Mean value of the drift rate MHz/s e_<Df> rms uncertainty on <Df> MHz/s <DfF> Fundamental band drift rate MHz/s <DfH> Harmonic band drift rate MHz/s l_Freq Limit flag on Freq --- Freq Frequence or upper value of frequence range MHz Freq2 Lower value of frequence when frequence range MHz <fH/fF> Mean value of the frequency ratio between the harmonic and fundamental band --- e_<fH/fF> rms uncertainty on <fH/fF> --- <fH/fF>u Upper value of the frequency ratio between the harmonic and fundamental band --- <fH/fF>l Lower value of the frequency ratio between the harmonic and fundamental band --- table1.tex TeX version of table1 table2.tex TeX version of table2 Patricia Bauer CDS 1996 May 10 G. Mann <gmann@aip.de> J_A+AS_119_489.xml Photometric distances to NGC 628 and its four companions J/A+AS/119/499 J/A+AS/119/499 NGC 628 and companions photometric distances Photometric distances to NGC 628 and its four companions M E Sharina I D Karachentsev N A Tikhonov Astron. Astrophys. Suppl. Ser. 119 499 1996 1996A&AS..119..499S Galaxies, photometry Redshifts galaxies: distances and redshifts galaxies: individual (NGC 628) galaxies: irregular Based on photometry of the brightest blue stars we derived distance moduli for NGC 628 and its dwarf irregular companions: DDO 13, UGC 1171, UGC 1104, and K 10. The mean modulus of the group is estimated to be 29.46 mag with a formal (internal) error of 0.11. The total mass to luminosity ratio of 40M_{sun}_/L_{sun}_ seems sufficient for NGC 628 to keep its companions in bound orbits.
NGC 628 01 36.7 +15 47 DDO 13 01 40.15 +15 56 UGC 1171 01 39.7 +15 54 UGC 1104 01 32.7 +18 19 UGCA 20 01 43.3 +19 59 NGC 660 01 43.0 +13 38 K68 10 01 43.7 +15 40
CCD photometry of the brightest stars in NGC628 Numb. Star number --- Xpos Rectangular coordinates of stars pix Ypos Rectangular coordinates of stars pix Vmag V magnitude mag B-V (B-V) colour index mag Notes By the letter "D" we indicate the cases when an object image appears diffuse. --- Photometry of stars in NGC628 Photometry of stars in DDO 13 Photometry of stars in UGC 1171 Photometry of stars in UGC 1104 Photometry of stars in K68 10 Brightest stars in UGCA 20 Star Star number --- Bmag B magnitude mag u_Bmag Uncertainty flag on B --- Vmag V magnitude mag Rmag R magnitude mag Properties of the galaxies around NGC 628 Galaxy Galaxy name --- MType Morphological type --- a Standard angular diameter arcmin b/a Apparent axis ratio --- Bt Total blue magnitude mag (B-V)0 Colour corrected for galactic extinction mag RVm Measured radial velocity km/s W50 HI line width measured at 50% level of maximum km/s RVc Radial velocity corrected for the Sun motion with respect to the Local Group centroid km/s Dist Measured distance Mpc NGC 628 and NGC 660 with their companions Galaxy Galaxy name --- A25 Standard linear diameter kpc (M/L)k Mass to luminosity ratio Sun Mk Mass of the galaxy 10+10solMass V1-Vk Velocity of the main galaxy minus velocity of its companion km/s R1k Projection of the linear separation between the galaxies kpc g1k Dimensionless potential factor --- t1k Cyclic orbital period of the companion measured in 1/H --- Patricia Bauer CDS 1996 May 06 Igor D.Karachentsev <ikar@sao.stavropol.su> J_A+AS_119_499.xml Atomic data from the IRON Project. XVII. Radiative transition probability for dipole allowed frobidden transitions in Fe III. J/A+AS/119/509 J/A+AS/119/509 IRON Project. XVII. Radiative transition in Fe III Atomic data from the IRON Project. XVII. Radiative transition probability for dipole allowed frobidden transitions in Fe III. S N Nahar A K Pradhan Astron. Astrophys. Suppl. Ser. 119 509 1996 1996A&AS..119..509N J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+A/293/953 : IRON Project VI. FeII collision strengths J/A+A/293/967 : IRON Project VII. FeII radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data infrared: general optical: general plasmas ultraviolet: general Table ls.dat contains all LS terms considered in this work and their energy values with complete designation. Table aij.dat contains f-, S-, and A-values of transitions, both in LS multiplet and in fine structure. For the full designation of the terms in the lower table check the top energy table. At the end of the lower table, a program in Fortran77 is written which can read the tables and calculate lifetime values from the A-values.
*LS terms Mul. Multiplet 1=Singlet, 3=Triplet, 5=Quintet, 7=Septets --- config Configuration --- n_SLpi Assigned degeneracy symbol --- SLpi Symmetry: (2S+1), L, parity of the term --- note State with * represents incomplete fs set --- D Degeneracy notation --- E(Ry,abs) Absolute energy Ry E(Ry,rel) Relative energy Ry Patricia Bauer CDS 1996 Mar 25 Sultana Nahar <nahar@payne.mps.ohio-state.edu> J_A+AS_119_509.xml Atomic data from the Iron Project. XVIII. Electron impact excitation collision strengths and rate coefficients for Fe III. J/A+AS/119/523 J/A+AS/119/523 IRON project XVIII. Fe III data Atomic data from the Iron Project. XVIII. Electron impact excitation collision strengths and rate coefficients for Fe III. H L Zhang Astron. Astrophys. Suppl. Ser. 119 523 1996 1996A&AS..119..523Z J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. FeII collision strengths J/A+A/293/967 : IRON Project VII. FeII radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data atomic processes The effective collision strengths upsilon coefficients are provided for FeIII (Z=26, 24 electrons) over the 23871 transitions between the 219 levels summarized in file 'levels', for the set of temperatures: 3000, 5000, 7000, 10000, 12000, 15000, 17000, 20000, 25000, 30000, 35000, 40000, 45000, 50000, 60000, 70000, 80000, 90000, and 100000 K.
Levels Index Level index --- Conf Electronic configuration --- Term Electronic term --- J Angular momentum --- E Theoretical energy Ry Patricia Bauer CDS 1996 Mar 25 Honglin Zhang <zhang@payne.mps.ohio-state.edu> J_A+AS_119_523.xml Stark broadening of Sr I spectral lines J/A+AS/119/529 J/A+AS/119/529 Stark broadening : Sr I Stark broadening of Sr I spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 119 529 1996 1996A&AS..119..529D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/367 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles Using a semiclassical approach, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for 33 Sr I multiplets for perturber densities 10^13^cm^-3^ (for stellar plasma research) and 10^15^-10^18^cm^-3^ (for laboratory plasma research) and temperatures T=2500-50000K.
Stark broadening parameters due to e-, p- and He II-impacts for Sr I N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for NV > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for NV > 0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe+ (4) --- WHe+ FWHM for He II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe+ (4) --- dHe+ shift for He II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1996 Apr 09 Milan Dimitrijevic <mdimitrijevic@aob.aob.bg.ac.yu> J_A+AS_119_529.xml Infrared aperture photometry at ESO (1983-1994) and its future use. J/A+AS/119/547 J/A+AS/119/547 IR photometry of ESO calibration stars Infrared aperture photometry at ESO (1983-1994) and its future use. N S Van der Bliek J Manfroid P Bouchet Astron. Astrophys. Suppl. Ser. 119 547 1996 1996A&AS..119..547V Infrared sources Photometry, infrared infrared: stars instrumentation: photometers techniques: photometric We describe the infrared (IR) photometric system for the single channel photometers at ESO, which have been used from 1983 until 1994. In addition to the broadband near infrared (NIR, 1-5{mu}m) photometric system presented in 1991 by Bouchet et al. and Bersanelli et al., we describe a narrow-band NIR photometric system and a mid infrared (MIR, 7-20{mu}m) photometric system. We also extend the set of NIR standard stars by Bouchet et al. towards fainter objects (K=~9). The photometric data of the standard stars in these systems were extracted from the complete IR photometric data archive of ESO, covering 10 years. The zeropoints of the NIR photometry are set by assuming that HR 3314 has a V-magnitude of 3.89, and that V-K=-0.05, J-K=-0.01, H-K=-0.01, K-L'=0.00, K-M=0.00. The zeropoints of the MIR photometry are set by assuming that the colours of{beta} Hyi (HR 0098) and {alpha} CenA (HR 5459) are equal to the colours of the Sun. We adopt the absolute calibration of Megessier (1995A&A...296..771M) for the NIR and we argue that this calibration can be extrapolated to 20{mu}m, using the MIR calibrations by Rieke et al. (1985AJ.....90..900R) and Cohen et al. (1992AJ....104.1650C). The definition of the zeropoints is consistent with the absolute calibration. We obtained accurate ({sigma}=~0.02mag.) NIR photometry of about 240 standard stars and MIR photometry of about 40 standard stars ({sigma}=~0.04mag). Comparison of our NIR photometric system with other well established systems shows that there are some small colour dependencies and zeropoint offsets which are always smaller than about 0.02mag. except for the L' band.
NIR (JHKL'M) broad band photometry of ESO calibration stars Name Star designation --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec Sp Spectral Type & Luminosity Class --- Jmag J magnitude (1.24 microns) mag e_Jmag Standard deviation of Jmag mag o_Jmag Number of observations in Jmag --- Hmag H magnitude (1.63 microns) mag e_Hmag Standard deviation of Hmag mag o_Hmag Number of observations in Hmag --- Kmag K magnitude (2.19 microns) mag e_Kmag Standard deviation of Kmag mag o_Kmag Number of observations in Kmag --- L'mag L' magnitude (3.79 microns) mag e_L'mag Standard deviation of L'mag mag o_L'mag Number of observations in L'mag --- Mmag M magnitude (4.64 microns) mag e_Mmag Standard deviation of Mmag mag o_Mmag Number of observations in Mmag --- MIR broad band photometry of ESO calibration stars Name Star designation --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec Sp Spectral Type & Luminosity Class --- H0 H_0 magnitude (1.58 microns) mag e_H0 Standard deviation of H_0 mag o_H0 Number of observations in H_0 --- BrGamma Br_gamma magnitude (2.16 microns) mag e_BrGamma Standard deviation of Br_gamma mag o_BrGamma Number of observations in Br_gamma --- K0 K_0 magnitude (2.22 microns) mag e_K0 Standard deviation of K_0 mag o_K0 Number of observations in K_0 --- CO CO magnitude (2.29 microns) mag e_CO Standard deviation of CO mag o_CO Number of observations in CO --- L0 L_0 magnitude (3.70 microns) mag e_L0 Standard deviation of L_0 mag o_L0 Number of observations in L_0 --- MIR photometry of ESO calibration stars Name Star designation --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec Sp Spectral Type & Luminosity Class --- Nmag N magnitude (10.36 microns) mag e_Nmag Standard deviation of Nmag mag o_Nmag Number of observations in Nmag --- N1 N1 magnitude (8.38 microns) mag e_N1 Standard deviation of N1 mag o_N1 Number of observations in N1 --- N2 N2 magnitude (9.69 microns) mag e_N2 Standard deviation of N2 mag o_N2 Number of observations in N2 --- N3 N3 magnitude (12.89 microns) mag e_N3 Standard deviation of N3 mag o_N3 Number of observations in N3 --- Q0 Q0 magnitude (18.06 microns) mag e_Q0 Standard deviation of Q0 mag o_Q0 Number of observations in Q0 --- Patricia Bauer CDS 1996 Apr 02 Nicole van der Bliek <nvdbliek@regge.strw.LeidenUniv.nl> J_A+AS_119_547.xml Transition probabilities for [Ni I] and [Ni II] lines. J/A+AS/119/99 J/A+AS/119/99 [Ni I] & [Ni II] transition probabilities Transition probabilities for [Ni I] and [Ni II] lines. P Quinet M Le Dourneuf Astron. Astrophys. Suppl. Ser. 119 99 1996 1996A&AS..119...99Q Atomic physics atomic data Ni I Ni II transition probabilities New radiative transition probabilities have been calculated for forbidden lines of astrophysical interest in Ni I and Ni II. The accuracy of the transition probability scales is established on the basis of two independent calculations performed with the approximately relativistic Hartree-Fock (HFR) and SUPERSTRUCTURE (SST) codes. Both physical models take into account the most important configuration interaction (CI) and relativistic effects.
Radiative transition probabilities, Aki in s-1, as obtained with HFR and SST for forbidden lines of Ni I. Multiplet Multiplet designation --- J-J' J-J' --- Lambda Predicted wavelengths from observed energy levels: see note number=1 Predicted wavelengths are deduced from the observed energy levels (Litzen et al. 1993). They are given in air above 200nm and in vacuum below 200nm. 0.1nm Type Type of transition --- Aki(HFR) HFR transition probabilities s-1 n_Aki(HFR) Comment on the HFR A-value: see note number=2 * Cancellation effects present. --- Aki(SST) SST transition probabilities s-1 Radiative transition probabilities, Aki in s-1, as obtained with HFR and SST for forbidden lines of Ni II. Multiplet Multiplet designation --- 2J-2J' 2J-2J' --- Lambda Predicted wavelengths from observed energy levels: see note number=1 Predicted wavelengths are deduced from the observed energy levels (Sugar and Corliss 1985). They are given in air above 200nm and in vacuum below 200nm. 0.1nm n_Lambda Comment on the wavelength: see note number=2 + Calculated HFR wavelength. --- Type Type of transition --- Aki(HFR) HFR transition probabilities s-1 n_Aki(HFR) Comment on the HFR A-value: see note number=3 * Cancellation effects present. --- Aki(SST) SST transition probabilities s-1 Patricia Bauer CDS 1996 Mar 25 Pascal Quinet <pascal@simpa3.univ-rennes1.fr> J_A+AS_119_99.xml CCD observations of Triton J/A+AS/120/107 J/A+AS/120/107 1989-1994 CCD observations of Triton CCD observations of Triton C H Veiga R Vieira Martins Astron. Astrophys. Suppl. Ser. 120 107 1996 1996A&AS..120..107V J/A+AS/131/291 : 1995-1997 CCD positions of Triton (Veiga+ 1998) Planets Positional data astrometry planets and satellites: general planets and satellites: individual (satellites of Neptune) Astrometric positions of the Neptunian Satellite Triton are given for the opposition of Neptune for the years 1989 to 1994. These positions where measured on 433 CCD frames obtained at the Cassegrain focus of a 1.6 m reflector. They are compared with theoretical positions calculated from Jacobson et al. (1991A&A...247..565J). The observed minus calculated residuals referred to Neptune have standard deviations of the order of 0.11".
List of observed positions of the Neptunian satellite Obs.Y Mean instant of the observation (year) yr Obs.M Mean instant of the observation (month) --- Obs.D Mean instant of the observation (day) d Sat Name of the satellite --- DRA {DELTA}{alpha}cos{delta} position relative to Neptune (1950.0) arcsec DDE {DELTA}{delta} position relative to Neptune (1950.0) arcsec Patricia Bauer CDS 1998 Mar 09 Carlos Henrique Veiga <cave@dans.on.br> J_A+AS_120_107.xml UBVRI photometric monitoring of 7 rapidly rotating late-type dwarfs in the Alpha Persei cluster J/A+AS/120/127 J/A+AS/120/127 UBVRI photometry of 7 dwarfs in Alpha Per UBVRI photometric monitoring of 7 rapidly rotating late-type dwarfs in the Alpha Persei cluster J Bouvier Astron. Astrophys. Suppl. Ser. 120 127 1996 1996A&AS..120..127B Photometry, UBVRI Stars, dwarfs open clusters and associations: individual (Alpha Per) stars: activity stars: late-type stars: magnetic fields stars: rotation The UBVRI light curves of 7 late-type dwarfs amongst the fastest rotators of the Alpha Per cluster (vsini>=140km/s) are presented. The shape of the light curves suggests that the photometric variations are most often dominated by a single group of cool spots located at intermediate or high latitude on the stellar surface. Assuming that starspots are good tracers of the stellar magnetic field, the smooth light curves indicate the existence of a large scale, slowly varying magnetic structure at the surface of these ultrafast rotators. For a description of the UBVRI photometric system, see e.g. <GCPD/08>
Alpha Persei cluster 03 22.0 +48 37
UBVRI photometry name Star name --- HJD Heliocentric Julian date d Mag Differential magnitude mag e_Mag rms error on the magnitude mag Color Filter --- Patricia Bauer CDS 1996 May 03 Jerome Bouvier <bouvier@cfht.hawaii.edu> J_A+AS_120_127.xml NTT V, I Colour-Magnitude Diagrams of the bulge globular cluster Tonantzintla 2 J/A+AS/120/153 J/A+AS/120/153 VI photometry of Ton 2 cluster NTT V, I Colour-Magnitude Diagrams of the bulge globular cluster Tonantzintla 2 E Bica S Ortolani B Barbuy Astron. Astrophys. Suppl. Ser. 120 153 1996 1996A&AS..120..153B Clusters, globular Photometry globular clusters: individual (Ton 2) Hertzsprung-Russell (HR diagram) Ton 2 is among the less-known Galactic globular clusters. We present for the first time colour magnitude diagrams in the V, I bands. We used the ESO NTT telescope under an excellent seeing of 0.6". The horizontal branch is red and close to the red giant branch, tilted by some differential reddening. The horizontal branch morphology and the red giant branch curvature suggest a metallicity similar to that of 47 Tucanae. We derive a reddening of E(B-V)=1.26 and a distance d_{sun}_=6.4kpc. Therefore, Ton 2 is =~2.0kpc from the Galactic center, and it appears to belong to the bulge population, being however only moderately metal rich.
Ton 2 Pismis 26 C 1732-385 07 38.1 +26 24
V, I photometry of Tonantzintla 2 No Sequence number --- Xpos X pixel coordinate as in Fig. 1 pix Ypos Y pixel coordinate as in Fig. 1 pix Vmag V magnitude mag V-I V-I color index mag Patricia Bauer CDS 1996 Apr 29 B. Barbuy <BARBUY@vax.iagusp.usp.br> J_A+AS_120_153.xml A compiled catalogue of optical positions of extragalactic radio sources. J/A+AS/120/201 J/A+AS/120/201 Extragalactic radio sources optical positions A compiled catalogue of optical positions of extragalactic radio sources. J Li W Jin Astron. Astrophys. Suppl. Ser. 120 201 1996 1996A&AS..120..201L J/A+AS/115/75 : Benchmark radio sources optical astrometry. III (Costa+, 1996) VII/54 : Extragalactic radio-source ident. cat. (Veron-Cetty+ 1983) I/218 : New Reference Frame defined by Extragalactic Radio Source (IAU WG, 1995) Galaxies, radio Positional data astrometry catalogs radio continuum: galaxies reference frames Based on 28 individual catalogues, in which the positions of optical counterparts of extragalactic radio sources are listed, we compiled a combined catalogue by means of a weighted least squares adjustment. The catalogue is in the system of FK5/J2000.0. It consists of about five hundred sources, among which there are 56 primary sources with position uncertainties as 0.09". Comparisons show that the orientation differences between optical and radio frames are A1=-0.013"+/-0.012", A2=0.077"+/-0.012", A3=0.005"+/-0.009". Local relative deformations are not obvious within the precision of ground-based optical observations.
The observations of optical counterparts of extragalactic radio sources Seq Sequential number --- Ref Reference author names --- BibCode Reference BibCode --- Nb Number of sources --- Dec1 Lower value of declination range deg Dec2 Upper value of declination range deg e_RAs rms uncertainty on right ascension s e_DEs rms uncertainty on declination arcsec Cat Catalogue of reference --- Ep Epoch of reference --- Relative rotations from each individual catalogue to the combined one Seq Sequential number --- Nb Number of sources --- A1 Relative rotation A1 arcsec e_A1 rms uncertainty on A1 arcsec A2 Relative rotation A2 arcsec e_A2 rms uncertainty on A2 arcsec A3 Relative rotation A3 arcsec e_A3 rms uncertainty on A3 arcsec Coordinates of primary sources in the compiled catalogue Source Source name (based on B1950 position) --- Status Status of the source (P: primary) --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec e_RAs rms uncertainty on right ascension s e_DEs rms uncertainty on declination arcsec IC Individual catalogue in which the source is available number=1 Each character corresponds to a sequential number of table1 --- TTS Type of the source number=2 Q: quasar B: BL Lac object G: galaxy --- mag Magnitude mag Name Other name --- James Marcout, Patricia Bauer CDS 1997 Sep 29 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_120_201.xml The distribution of ionized gas in early-type galaxies. II. The velocity field of the ionized gas J/A+AS/120/257 J/A+AS/120/257 Ionized gas velocity in 6 galaxies The distribution of ionized gas in early-type galaxies. II. The velocity field of the ionized gas W W Zeilinger A Pizzella P Amico G Bertin F Bertola L M Buson I J Danziger H Dejonghe E M Sadler R P Saglia P T de Zeeuw Astron. Astrophys. Suppl. Ser. 120 257 1996 1996A&AS..120..257Z Galaxies, spectra Radial velocities galaxies: elliptical and lenticular, cD galaxies: ISM galaxies: structure We report observations of the velocity field of the ionized gas in the nearby ellipticals NGC 1453, NGC 2974, NGC 3962, NGC 4636, NGC 6868 and NGC 7097. This is part of an ESO Key Programme intended to derive the mass distribution of elliptical galaxies and to investigate the possible presence of dark matter. All galaxy spectra are characterized by LINER-type emission. The derived gas kinematics confirm the picture of a regular gaseous disk structure with ordered rotation. The gas velocity dispersion profiles decline rapidly from a high central value in the range of =~150 to =~250km/s.
NGC 1453 03 46.4 -03 57 NGC 2974 09 42.5 -03 42 NGC 3962 11 54.7 -13 58 NGC 4636 12 42.9 +02 42 NGC 6868 20 09.9 -48 23 NGC 7097 21 40.2 -42 32
Radial velocities for NGC 1453 rad0b PA=000 (3.6m) radius arcsec RV0b PA=000 (3.6m) radial velocity km/s rad20 PA=020 (2.2m) radius arcsec RV20 PA=020 (2.2m) radial velocity km/s rad45b PA=045 (3.6m) radius arcsec RV45b PA=045 (3.6m) radial velocity km/s rad45 PA=045 (2.2m) radius arcsec RV45 PA=045 (2.2m) radial velocity km/s rad90b PA=090 (3.6m) radius arcsec RV90b PA=090 (3.6m) radial velocity km/s rad90 PA=090 (2.2m) radius arcsec RV90 PA=090 (2.2m) radial velocity km/s rad110 PA=110 (2.2m) radius arcsec RV110 PA=110 (2.2m) radial velocity km/s rad135b PA=135 (3.6m) radius arcsec RV135b PA=135 (3.6m) radial velocity km/s rad165 PA=165 (2.2m) radius arcsec RV165 PA=165 (2.2m) radial velocity km/s Radial velocities for NGC 2974 rad0b PA=000 (3.6m) radius arcsec RV0b PA=000 (3.6m) radial velocity km/s rad25b PA=025 (3.6m) radius arcsec RV25b PA=025 (3.6m) radial velocity km/s rad45r PA=045 (3.6m rebinned) radius arcsec RV45r PA=045 (3.6m rebinned) radial velocity km/s rad70b PA=070 (3.6m) radius arcsec RV70b PA=070 (3.6m) radial velocity km/s rad90b PA=090 (3.6m) radius arcsec RV90b PA=090 (3.6m) radial velocity km/s rad90r PA=090 (3.6m rebinned) radius arcsec RV90r PA=090 (3.6m rebinned) radial velocity km/s rad115b PA=115 (3.6m) radius arcsec RV115b PA=115 (3.6m) radial velocity km/s rad135b PA=135 (3.6m) radius arcsec RV135b PA=135 (3.6m) radial velocity km/s rad135r PA=135 (3.6m rebinned) radius arcsec RV135r PA=135 (3.6m rebinned) radial velocity km/s rad160b PA=160 (3.6m) radius arcsec RV160b PA=160 (3.6m) radial velocity km/s Radial velocities for NGC 3962 rad10b PA=010 (3.6m) radius arcsec RV10b PA=010 (3.6m) radial velocity km/s rad10 PA=010 (2.2m) radius arcsec RV10 PA=010 (2.2m) radial velocity km/s rad30r PA=030 (3.6m rebinned) radius arcsec RV30r PA=030 (3.6m rebinned) radial velocity km/s rad30 PA=030 (2.2m) radius arcsec RV30 PA=030 (2.2m) radial velocity km/s rad40b PA=040 (3.6m) radius arcsec RV40b PA=040 (3.6m) radial velocity km/s rad70b PA=070 (3.6m) radius arcsec RV70b PA=070 (3.6m) radial velocity km/s rad70r PA=070 (3.6m rebinned) radius arcsec RV70r PA=070 (3.6m rebinned) radial velocity km/s rad100b PA=100 (3.6m) radius arcsec RV100b PA=100 (3.6m) radial velocity km/s rad100r PA=130 (3.6m rebinned) radius arcsec RV100r PA=130 (3.6m rebinned) radial velocity km/s rad130 PA=130 (2.2m) radius arcsec RV130 PA=130 (2.2m) radial velocity km/s rad160b PA=160 (3.6m) radius arcsec RV160b PA=160 (3.6m) radial velocity km/s Radial velocities for NGC 4636 rad0b PA=000 (3.6m) radius arcsec RV0b PA=000 (3.6m) radial velocity km/s rad15 PA=015 (2.2m) radius arcsec RV15 PA=015 (2.2m) radial velocity km/s rad30b PA=030 (3.6m) radius arcsec RV30b PA=030 (3.6m) radial velocity km/s rad45 PA=045 (2.2m) radius arcsec RV45 PA=045 (2.2m) radial velocity km/s rad60b PA=060 (3.6m) radius arcsec RV60b PA=060 (3.6m) radial velocity km/s rad85 PA=085 (2.2m) radius arcsec RV85 PA=085 (2.2m) radial velocity km/s rad90b PA=090 (3.6m) radius arcsec RV90b PA=090 (3.6m) radial velocity km/s rad90 PA=090 (2.2m) radius arcsec RV90 PA=090 (2.2m) radial velocity km/s rad105b PA=105 (3.6m) radius arcsec RV105b PA=105 (3.6m) radial velocity km/s rad120b PA=120 (3.6m) radius arcsec RV120b PA=120 (3.6m) radial velocity km/s rad135b PA=135 (3.6m) radius arcsec RV135b PA=135 (3.6m) radial velocity km/s rad135 PA=135 (2.2m) radius arcsec RV135 PA=135 (2.2m) radial velocity km/s rad150b PA=150 (3.6m) radius arcsec RV150b PA=150 (3.6m) radial velocity km/s Radial velocities for NGC 6868 rad10b PA=010 (3.6m) radius arcsec RV10b PA=010 (3.6m) radial velocity km/s rad30b PA=030 (3.6m) radius arcsec RV30b PA=030 (3.6m) radial velocity km/s rad60b PA=060 (3.6m) radius arcsec RV60b PA=060 (3.6m) radial velocity km/s rad80b PA=080 (3.6m) radius arcsec RV80b PA=080 (3.6m) radial velocity km/s rad110r PA=110 (3.6m rebinned) radius arcsec RV110r PA=110 (3.6m rebinned) radial velocity km/s rad120b PA=120 (3.6m) radius arcsec RV120b PA=120 (3.6m) radial velocity km/s rad150 PA=150 (2.2m) radius arcsec RV150 PA=150 (2.2m) radial velocity km/s rad170b PA=170 (3.6m) radius arcsec RV170b PA=170 (3.6m) radial velocity km/s Radial velocities for NGC 7097 rad10 PA=000 (2.2m) radius arcsec RV10 PA=000 (2.2m) radial velocity km/s rad20 PA=020 (2.2m) radius arcsec RV20 PA=020 (2.2m) radial velocity km/s rad45 PA=045 (2.6m) radius arcsec RV45 PA=045 (2.2m) radial velocity km/s rad90 PA=090 (2.2m) radius arcsec RV90 PA=090 (2.2m) radial velocity km/s rad110 PA=110 (2.2m) radius arcsec RV110 PA=110 (2.2m) radial velocity km/s Radial velocity dispersions for NGC 1453 rad0b PA=000 (3.6m) radius arcsec sigma0b PA=000 (3.6m) radial velocity dispersion km/s rad20 PA=020 (2.2m) radius arcsec sigma20 PA=020 (2.2m) radial velocity dispersion km/s rad45b PA=045 (3.6m) radius arcsec sigma45b PA=045 (3.6m) radial velocity dispersion km/s rad45 PA=045 (2.2m) radius arcsec sigma45 PA=045 (2.2m) radial velocity dispersion km/s rad90b PA=090 (3.6m) radius arcsec sigma90b PA=090 (3.6m) radial velocity dispersion km/s rad90 PA=090 (2.2m) radius arcsec sigma90 PA=090 (2.2m) radial velocity dispersion km/s rad110 PA=110 (2.2m) radius arcsec sigma110 PA=110 (2.2m) radial velocity dispersion km/s rad135b PA=135 (3.6m) radius arcsec sigma135b PA=135 (3.6m) radial velocity dispersion km/s rad165 PA=165 (2.2m) radius arcsec sigma165 PA=165 (2.2m) radial velocity dispersion km/s Radial velocity dispersions for NGC 2974 rad0b PA=000 (3.6m) radius arcsec sigma0b PA=000 (3.6m) radial velocity dispersion km/s rad25b PA=025 (3.6m) radius arcsec sigma25b PA=025 (3.6m) radial velocity dispersion km/s rad45r PA=045 (3.6m rebinned) radius arcsec sigma45r PA=045 (3.6m rebinned) radial velocity disp. km/s rad70b PA=070 (3.6m) radius arcsec sigma70b PA=070 (3.6m) radial velocity dispersion km/s rad90b PA=090 (3.6m) radius arcsec sigma90b PA=090 (3.6m) radial velocity dispersion km/s rad90r PA=090 (3.6m rebinned) radius arcsec sigma90r PA=090 (3.6m rebinned) radial velocity disp. km/s rad115b PA=115 (3.6m) radius arcsec sigma115b PA=115 (3.6m) radial velocity dispersion km/s rad135b PA=135 (3.6m) radius arcsec sigma135b PA=135 (3.6m) radial velocity dispersion km/s rad135r PA=135 (3.6m rebinned) radius arcsec sigma135r PA=135 (3.6m rebinned) radial velocity disp. km/s rad160b PA=160 (3.6m) radius arcsec sigma160b PA=160 (3.6m) radial velocity dispersion km/s Radial velocity dispersions for NGC 3962 rad10b PA=010 (3.6m) radius arcsec sigma10b PA=010 (3.6m) radial velocity dispersion km/s rad10 PA=010 (2.2m) radius arcsec sigma10 PA=010 (2.2m) radial velocity dispersion km/s rad30r PA=030 (3.6m rebinned) radius arcsec sigma30r PA=030 (3.6m rebinned) radial velocity disp. km/s rad30 PA=030 (2.2m) radius arcsec sigma30 PA=030 (2.2m) radial velocity dispersion km/s rad40b PA=040 (3.6m) radius arcsec sigma40b PA=040 (3.6m) radial velocity dispersion km/s rad70b PA=070 (3.6m) radius arcsec sigma70b PA=070 (3.6m) radial velocity dispersion km/s rad70r PA=070 (3.6m rebinned) radius arcsec sigma70r PA=070 (3.6m rebinned) radial velocity disp. km/s rad100b PA=100 (3.6m) radius arcsec sigma100b PA=100 (3.6m) radial velocity dispersion km/s rad130r PA=130 (3.6m rebinned) radius arcsec sigma130r PA=130 (3.6m rebinned) radial velocity disp. km/s rad130 PA=130 (2.2m) radius arcsec sigma130 PA=130 (2.2m) radial velocity dispersion km/s rad160b PA=160 (3.6m) radius arcsec sigma160b PA=160 (3.6m) radial velocity dispersion km/s Radial velocity dispersions for NGC 4636 rad0b PA=000 (3.6m) radius arcsec sigma0b PA=000 (3.6m) radial velocity dispersion km/s rad15 PA=015 (2.2m) radius arcsec sigma15 PA=015 (2.2m) radial velocity dispersion km/s rad30b PA=030 (3.6m) radius arcsec sigma30b PA=030 (3.6m) radial velocity dispersion km/s rad45 PA=045 (2.2m) radius arcsec sigma45 PA=045 (2.2m) radial velocity dispersion km/s rad60b PA=060 (3.6m) radius arcsec sigma60b PA=060 (3.6m) radial velocity dispersion km/s rad85 PA=085 (2.2m) radius arcsec sigma85 PA=085 (2.2m) radial velocity dispersion km/s rad90b PA=090 (3.6m) radius arcsec sigma90b PA=090 (3.6m) radial velocity dispersion km/s rad90 PA=090 (2.2m) radius arcsec sigma90 PA=090 (2.2m) radial velocity dispersion km/s rad105b PA=105 (3.6m) radius arcsec sigma105b PA=105 (3.6m) radial velocity dispersion km/s rad120b PA=120 (3.6m) radius arcsec sigma120b PA=120 (3.6m) radial velocity dispersion km/s rad135b PA=135 (3.6m) radius arcsec sigma135b PA=135 (3.6m) radial velocity dispersion km/s rad135 PA=135 (2.2m) radius arcsec sigma135 PA=135 (2.2m) radial velocity dispersion km/s rad150b PA=150 (3.6m) radius arcsec sigma150b PA=150 (3.6m) radial velocity dispersion km/s Radial velocity dispersions for NGC 6868 rad10b PA=010 (3.6m) radius arcsec sigma10b PA=010 (3.6m) radial velocity dispersion km/s rad30b PA=030 (3.6m) radius arcsec sigma30b PA=030 (3.6m) radial velocity dispersion km/s rad60b PA=060 (3.6m) radius arcsec sigma60b PA=060 (3.6m) radial velocity dispersion km/s rad80b PA=080 (3.6m) radius arcsec sigma80b PA=080 (3.6m) radial velocity dispersion km/s rad110 PA=110 (2.2m) radius arcsec sigma110 PA=110 (2.2m) radial velocity dispersion km/s rad120b PA=120 (3.6m) radius arcsec sigma120b A=120 (3.6m) radial velocity dispersion km/s rad150 PA=150 (2.2m) radius arcsec sigma150 PA=150 (2.2m) radial velocity dispersion km/s rad170b PA=170 (3.6m) radius arcsec sigma170b PA=170 (3.6m) radial velocity dispersion km/s Radial velocity dispersions for NGC 7097 rad0 PA=000 (2.2m) radius arcsec sigma0 PA=000 (2.2m) radial velocity dispersion km/s rad20 PA=020 (2.2m) radius arcsec sigma20 PA=020 (2.2m) radial velocity dispersion km/s rad45 PA=045 (2.2m) radius arcsec sigma45 PA=045 (2.2m) radial velocity dispersion km/s rad90 PA=090 (2.2m) radius arcsec sigma90 PA=090 (2.2m) radial velocity dispersion km/s rad110 PA=110 (2.2m) radius arcsec sigma110 PA=110 (2.2m) radial velocity dispersion km/s Patricia Bauer CDS 1996 May 23 J_A+AS_120_257.xml Light curves and periods of Mira variables J/A+AS/120/275 J/A+AS/120/275 Mira variables light curves Light curves and periods of Mira variables C Alard A Terzan J Guibert Astron. Astrophys. Suppl. Ser. 120 275 1996 1996A&AS..120..275A Photometry Stars, variable Galaxy: center infrared: stars stars: AGB and post-AGB Good distance indicators are needed in studies of the galactic structure. Pulsating variables can be used, but the problem is to find a homogeneous sample obeying a period-luminosity relation with low scatter. In this paper, we show how such a sample can be produced using the Terzan catalogue of Variables and available Schmidt plates. We have selected 150 large amplitude variables discovered by Terzan in a field of 25 sq degrees near the Galactic Centre. A set of 22 red plates was scanned with the MAMA machine, providing time series for all the variables. The times series were analysed using both the periodogram and Renson's method. Periods could be derived for 122 stars of the sample showing clearly that most of these objects are Miras. As a conclusion we show that with some infrared photometry, these Miras could be used as good distance indicators in this region.
Coordinates, periods and R magnitudes of the Mira variables Terzan Terzan number number=1 Terzan number: see Terzan, A., Bijaoui, A., Ju, K.H., Ounnas, C. 1982A&AS...49..715T = Cat. <J/A+AS/49/715> --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec GLON Galactic longitude lII deg GLAT Galactic latitude bII deg P Period d Rmagmax R magnitude at maximum mag Rmagmin R magnitude at minimum number=2 The "R magnitude at minimum" is, for some stars, imposed by the faintest standard available for the calibration. mag Note Notes --- Patricia Bauer CDS 1996 Jul 26 Jean Guibert <Guibert@mesiob.obspm.fr> J_A+AS_120_275.xml A survey of water maser emission toward ultracompact HII regions J/A+AS/120/283 J/A+AS/120/283 Water maser features in ultracompact HII regions A survey of water maser emission toward ultracompact HII regions P Hofner E Churchwell Astron. Astrophys. Suppl. Ser. 120 283 1996 1996A&AS..120..283H Masers Radio lines HII regions masers radio lines: ISM In this paper we present high resolution images and spectra toward 21 H_2_O maser sources in the vicinity of ultracompact (UC) HII regions. This survey provides the basis for future studies with milli-arcsecond resolution, utilizing very long baseline interferometry (VLBI) techniques. Emission from the 6_16_-5_23_ masing transition of interstellar H_2_O is observed in the close vicinity of UC HII regions with a median angular distance of 2.9" and a median linear projected distance of 0.1pc from the continuum peak. We find that for UC HII regions with cometary morphology the water maser emission is located in front of the cometary arc whereas for non-cometary UC HII regions the water masers are often observed projected onto the contours of the ionized gas. Due to the large median distance of the water masers from the I-front of the UC HII region, it is unlikely, that the water masers are formed in the shocked layer of warm molecular gas in the interface between the ionized gas of the UC HII region and surrounding molecular gas which is predicted by the Bow Shock theory of UC HII regions. A comparison with maps in the NH_3_ inversion transitions shows that in at least 7 cases, the water masers are associated with hot (T>100K), dense (n(H_2_)=~10^7^cm^-3^) molecular clumps. For the UC HII regions G5.89-0.38 and G45.07+0.13 we find spatial and velocity correspondence between water masers and outflowing molecular gas. It is thus likely, that for these sources the H_2_O masers are taking part in the bipolar outflow.
Observed water maser features Soure Source name --- No Number of maser cluster --- m_No Multiplicity index on No --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vlsr LSR velocity of feature km/s Inu Intensity of feature (Jy/beam) Jy DeltaV Velocity range over which emission is observed in the cluster km/s n_DeltaV Note number=1 a: Full Width at Zero Power for single features b: Distance to UC HII region >20" --- table3.tex TeX version of table3 Patricia Bauer CDS 1996 May 09 P. Hofner <hofner@ph1.Uni-Koeln.DE> J_A+AS_120_283.xml Dust colors, dust release rates, and dust-to-gas ratios in the comae of six comets. J/A+AS/120/301 J/A+AS/120/301 Comae of six comets Dust colors, dust release rates, and dust-to-gas ratios in the comae of six comets. G C Sanzovo P D Singh W F Huebner Astron. Astrophys. Suppl. Ser. 120 301 1996 1996A&AS..120..301S Comets comets: general comets: individual (Bowell 1982 I, Bradfield 1979 X) comets: individual (Brorsen-Metcalf 1989 X) comets: individual (Giacobini-Zinner 1985 XII) comets: individual (Levy 1990 XX, Stephan-Oterma 1980 X) In an attempt to find correlations between properties of comets, we determine the dust colors, dust release rates, and dust-to-gas mass ratios in the comae of Comets Bowell (1980b=1982I), Bradfield (1979l=1979X), Brorsen-Metcalf (1989o=1989X), Giacobini-Zinner (1984e=1985XIII), Levy (1990c=1990XX), and Stephan-Oterma (1980g=1980X) using a uniform and systematic analysis of the continuum fluxes measured at optical wavelengths. We assume that the continuum fluxes observed in these comets are from light scattered by micrometer-sized dust particles. The color of the dust is blue, relative to the Sun, in Comets Bradfield (1979 X) and Brorsen-Metcalf (1989 X); both comets have a low dust-to-gas mass ratio ({chi}<10%). Comets Giacobini-Zinner (1985 XIII) and Stephan-Oterma (1980 X) have an intermediate dust-to-gas mass ratio (10%<{chi}<40%), whereas Comets Levy (1990 XX) and Bowell (1982 I) have a high dust-to-gas mass ratio ({chi}>40%). The continuum flux from dust particles in comets with intermediate to high dust-to-gas mass ratios is in general red, relative to the Sun. However, the color changes to blue in these comets when the dust-to-gas mass ratios are low relative to their peak values. ************************************************************************** * * * Sorry, but the author(s) did not provide their tables as announced * * in the paper * * * **************************************************************************
Patricia Bauer CDS 1996 May 24 J_A+AS_120_301.xml Observations of a complete sample of H{alpha} emission-line galaxies. Long-slit spectroscopy of galaxies in UCM lists 1 and 2 J/A+AS/120/323 J/A+AS/120/323 Long-slit spectroscopy of UCM galaxies Observations of a complete sample of H{alpha} emission-line galaxies. Long-slit spectroscopy of galaxies in UCM lists 1 and 2 J Gallego J Zamorano M Rego O Alonso A G Vitores Astron. Astrophys. Suppl. Ser. 120 323 1996 1996A&AS..120..323G Galaxies, spectra galaxies: distances and redshifts galaxies: starburst surveys Spectroscopic observations for the full sample of H{alpha} emission-line galaxy candidates (ELGs) from the Universidad Complutense de Madrid objective-prism survey Lists 1 and 2 have been obtained in order to investigate fully the properties of the survey constituents as well as the selection characteristics and completeness limits of the survey itself. The spectroscopic data include redshifts, line fluxes, equivalent widths, emission-line ratios, optical reddening estimates and synthesized color indexes. We find that 74% of the objects in this sample do exhibit emission lines. We compare our observational data with parameters given in the published survey lists in order to assess the usefulness of the latter. The different emission-line galaxies have been classified according to their spectra in several groups. Gray-scale images of the CCD spectra near the main emission lines, spatial profiles at the continuum and the line for [OIII]{lambda}5007 and H{alpha} lines, as well as plots of the coadded spectra of selected galaxies are presented, and a number of peculiar objects are described.
Summary of emission-line intensities UCM UCM name (Zamorano et al., 1994ApJS...95..387Z) --- m_UCM Multiplicity index on UCM --- [OII] [OII]{lambda}3727 number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % Hgamma Hgamma{lambda}4340 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % Hbeta Hbeta{lambda}4861 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [OIII]a [OIII]{lambda}4959 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [OIII]b [OIII]{lambda}5007 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % HeI HeI{lambda}5976 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [OI] [OI]{lambda}6300 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [NII]a [NII]{lambda}6548 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % Halpha Halpha{lambda}6563 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [NII]b [NII]{lambda}6584 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [SII]a line flux of [SII]{lambda}6716 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [SII]b line flux of [SII]{lambda}6731 line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [OII]c Reddening-corrected [OII] line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % Hgammac Reddening-corrected Hgamma line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % Hbetac Reddening-corrected Hbeta line flux (=100) % [OIII]ac Reddening-corrected [OIII](4959A) line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [OIII]bc Reddening-corrected [OIII](5007A) line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % HeIc Reddening-corrected HeI line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [OI]c Reddening-corrected [OI] line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [NII]ac Reddening-corrected [NII](6548A) line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % Halphac Reddening-corrected Halpha line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [NII]bc Reddening-corrected [NII](6584A) line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [SII]ac Reddening-corrected [SII](6716A) line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % [SII]bc Reddening-corrected [SII](6731A) line flux number=1 Line fluxes are relative to Hbeta=100 for all emission lines detected. In case of no Hbeta line apparent, the fluxes are given relatives to Halpha=100. % Summary of spectroscopic data UCM Name in Zamorano+, 1994ApJS...95..387Z --- m_UCM Multiplicity index on UCM --- z Heliocentric redshift --- SNR Signal-to-noise ratio at the continuum near Halpha number=1 SNR estimated by computing the ratio between the sigma in a 10nm band centered at 6540Angstroem (rest wavelength) and the mean flux in the same range --- EW([OII]) Equivalent width for [OII]{lambda}3727 emission line 0.1nm EW(Hbeta) Equivalent width for Hbeta emission line 0.1nm EW([OIII]) Equivalent width for [OIII]{lambda}5007 emission line 0.1nm EW(Halpha) Equivalent width for Halpha emission line 0.1nm FHbeta Observed Hbeta line flux 10-17W/m2 FHalpha Observed blend Halpha+[NII] line flux 10-17W/m2 b-v b-v synthetic color index mag v-r v-r synthetic color index mag E(B-V) B-V color excess mag u_E(B-V) Uncertainty flag on E(B-V) --- L(Halpha) Observed Halpha luminosity 10+8solLum Spect Spectroscopic classification --- table4.tex LaTeX version of table4 table5.tex LaTeX version of table5 Patricia Bauer CDS 1996 May 21 Jesus Gallego <jgm@ucolick.org> J_A+AS_120_323.xml CCD Sequences in the Shapley supercluster of Galaxies. I. The LCO-Toronto telescope data. J/A+AS/120/357 J/A+AS/120/357 R magnitudes in four ESO fields CCD Sequences in the Shapley supercluster of Galaxies. I. The LCO-Toronto telescope data. L Infante E Slezak H Quintana Astron. Astrophys. Suppl. Ser. 120 357 1996 1996A&AS..120..357I Clusters, galaxy Photometry, CCD galaxies: photometry surveys techniques: photometric We present R CCD photometric sequences of stars for calibrating ESO/SERC(R) survey plates in the region of the Shapley supercluster of galaxies.
All results as a single file. Field ESO field number --- Spot Spot designation --- No Rank number in the catalogue. --- RAh Right ascension of the object (equinox 2000.0) h RAm Right ascension of the object (equinox 2000.0) min RAs Right ascension of the object (equinox 2000.0) s DE- Declination sign --- DEd Declination of the object (equinox 2000.0) deg DEm Declination of the object (equinox 2000.0) arcmin DEs Declination of the object (equinox 2000.0) arcsec Rmag Magnitude in the R band mag R photometry of 9 objects in ESO field 382, spot C' R photometry of 16 objects in ESO field 382, spot F' R photometry of 23 objects in ESO field 382, spot G' R photometry of 22 objects in ESO field 382, spot K' R photometry of 15 objects in ESO field 382, spot L' R photometry of 15 objects in ESO field 383, spot G' R photometry of 17 objects in ESO field 383, spot K' R photometry of 23 objects in ESO field 383, spot L' R photometry of 13 objects in ESO field 443, spot M' R photometry of 13 objects in ESO field 443, spot M" R photometry of 14 objects in ESO field 444, spot D' R photometry of 15 objects in ESO field 444, spot E' R photometry of 6 objects in ESO field 444, spot G' R photometry of 17 objects in ESO field 444, spot K' R photometry of 18 objects in ESO field 444, spot L' No Rank number in the catalogue. --- RAh Right ascension of the object (equinox 2000.0) h RAm Right ascension of the object (equinox 2000.0) min RAs Right ascension of the object (equinox 2000.0) s DE- Declination sign --- DEd Declination of the object (equinox 2000.0) deg DEm Declination of the object (equinox 2000.0) arcmin DEs Declination of the object (equinox 2000.0) arcsec Rmag Magnitude in the R band mag Patricia Bauer CDS 1996 Apr 24 Eric Slezak, <slezak@purcell.obs-nice.fr> J_A+AS_120_357.xml Atomic data from the IRON Project. XIX. Radiative transition probabilities for forbidden lines in Fe II J/A+AS/120/361 J/A+AS/120/361 IRON Project. XIX. Fe II radiative transitions Atomic data from the IRON Project. XIX. Radiative transition probabilities for forbidden lines in Fe II P Quinet M Le Dourneuf C J Zeippen Astron. Astrophys. Suppl. Ser. 120 361 1996 1996A&AS..120..361Q J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths Atomic physics atomic data Fe II transition probabilities Radiative transition probabilities have been calculated for the magnetic dipole (M1) and electric quadrupole (E2) transitions connecting the 63 metastable levels in the 3d64s, 3d7 and 3d54s2 configurations in Fe II. The most important configuration interaction (CI) and relativistic effects have been taken into account in the computations carried out with the help of two independent computer programs, SUPERSTRUCTURE (SST) and RELATIVISTIC HARTREE-FOCK (HFR). The results obtained in the present work are compared with previous theoretical studies and with some astrophysical observations. The new data presented here are probably the most reliable to date.
Radiative transition probabilities, Aki in s-1, as obtained with SST and HFR for forbidden lines of Fe II. Multiplet Multiplet --- 2J-2J' 2J-2J' --- Lambda Predicted wavelengths from observed energy levels number=1 Predicted wavelengths, given in air, are deduced from the observed energy levels compiled by Sugar & Corliss (1985, J. Phys. Chem. Ref. Data 14, Suppl. 2). 0.1nm Type Type of transition --- Aki(SST) SST transition probabilities s-1 Aki(HFR) HFR transition probabilities s-1 --- Comment on the HFR A-value number=2 * Cancellation effects present. --- Patricia Bauer CDS 1997 Jan 10 Pascal Quinet <pascal@simpa3.univ-rennes1.fr> J_A+AS_120_361.xml Stark width for astrophysically important ns-np transitions in Sc II, Y II and Zr II spectra. J/A+AS/120/373 J/A+AS/120/373 Sc II, Y II & Zr II Stark width Stark width for astrophysically important ns-np transitions in Sc II, Y II and Zr II spectra. L C Popovic M S Dimitrijevic Astron. Astrophys. Suppl. Ser. 120 373 1996 1996A&AS..120..373P VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles Here we present Stark widths for some astrophysically important ns-np transitions of Sc II, Y II and Zr II. Stark widths were calculated within the modified semiempirical approach. The obtained results were compared with simple estimates based on regularities and systematic trends.
*Stark full width (FWHM) for Sc II, Y II and Zr II spectral lines Ion Ion --- Trans Transition --- Lambda Wavelength nm n_Lambda a stands for averaged wavelength of the multiplet --- T Temperature K W Stark width nm tables.tex TeX version of table1-3 Patricia Bauer CDS 1996 May 24 Dr. Luka C. Popovic <lpopovic@aob.bg.ac.yu> J_A+AS_120_373.xml 1.65 micron (H-band) surface photometry of galaxies. I: Observations of 158 galaxies with the Calar Alto 2.2m telescope. J/A+AS/120/489 J/A+AS/120/489 Galaxies morphology and IR photometry I. 1.65 micron (H-band) surface photometry of galaxies. I: Observations of 158 galaxies with the Calar Alto 2.2m telescope. G Gavazzi D Pierini A Boselli R Tuffs Astron. Astrophys. Suppl. Ser. 120 489 1996 1996A&AS..120..489G J/A+AS/120/521 : Galaxies morphology and IR photometry II. (Gavazzi+ 1996) Morphology Photometry, infrared Photometry, surface galaxies: fundamental parameters galaxies: photometry infrared: galaxies Near Infrared (H-band) surface photometry of 158 (mostly) disk galaxies belonging to the Coma Supercluster and to the A262 and Cancer clusters was obtained using the 256^2^ NICMOS3 array MAGIC attached to the 2.2m Calar Alto telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices and total H magnitudes are derived.
Parameters of the galaxies observed at Calar Alto CGCG CGCG denominations (Catalogue <VII/49>) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Memb Cluster membership --- MType Morphological type --- a25 Major optical diameter (a_25) arcmin b25 Minor optical diameter (b_25) arcmin mpg CGCG magnitude, photographic or J mag n_mpg J when mpg is a J magnitude --- Hmag Total H magnitude (H_T) mag Year-1900 Observing year (1900+) yr Year2-1900 Second year when two years yr Rem Remarks --- Photometric parameters for the galaxies observed at Calar Alto. CGCG CGCG denominations (Catalogue <VII/49>) --- Date Observing dates (day-month-year) --- Size Pixel size arcsec Int.T Total integration time (N_c x t_int x N_f) number=1 The total integration time is written as the product of the number of coadds N_c, the on-chip integration time t_int, and the number of frames N_f combined to form the final image. s Phot Photometric quality (*=non-photometric) --- PA Position Angle (measured counterclockwise from N) deg Eps Ellipticity (1-b/a) --- a21.5 Galaxy major radius arcsec H21.5 Observed magnitudes mag C31 Concentration index C_31 --- Patricia Bauer CDS 1996 May 31 Giuseppe Peppo Gavazzi <gavazzi@brera.mi.astro.it> J_A+AS_120_489.xml 1.65 micron (H-band) surface photometry of galaxies. II: observations of 297 galaxies with the TIRGO 1.5m telescope. J/A+AS/120/521 J/A+AS/120/521 Galaxies morphology and IR photometry II. 1.65 micron (H-band) surface photometry of galaxies. II: observations of 297 galaxies with the TIRGO 1.5m telescope. G Gavazzi D Pierini C Baffa F Lisi L K Hunt I Randone A Boselli Astron. Astrophys. Suppl. Ser. 120 521 1996 1996A&AS..120..521G J/A+AS/120/489 : Galaxies morphology and IR photometry I. (Gavazzi+ 1996) Morphology Photometry, surface galaxies: fundamental parameters galaxies: photometry infrared: galaxies We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, <J/A+AS/120/489>) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. <GCPD/59>
Parameters of the galaxies observed at TIRGO. CGCG CGCG denominations (Catalogue <VII/49>) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Memb Cluster membership --- MType Morphological type --- a25 Major optical diameter (a_25) arcmin b25 Minor optical diameter (b_25) arcmin mpg CGCG photographic magnitude mag Hmag Total H magnitude (H_T) mag Date Observing year. yr Photometric parameters for the galaxies observed at TIRGO CGCG CGCG denominations (Catalogue <VII/49>) --- Date Observing dates (day-month-year) --- Int.T Total integration time (N_c x t_int x N_f) number=1 The total integration time is written as the product of the number of coadds N_c, the on-chip integration time t_int, and the number of frames N_f combined to form the final image. s Phot Photometric quality (*=non-photometric) --- PA Position Angle (measured counterclockwise from N) deg Eps Ellipticity (1-b/a) --- a21.5 Galaxy major radius arcsec n_a21.5 "noiser than average" flag --- H21.5 Observed magnitudes mag n_H21.5 "noiser than average" flag --- C31 Concentration index C_31 --- n_C31 "noiser than average" flag --- Patricia Bauer CDS 1996 May 31 Giuseppe Peppo Gavazzi <gavazzi@brera.mi.astro.it> J_A+AS_120_521.xml A radio continuum study of the Magellanic Clouds. Part IVa: Catalogues of radio sources in the Large Magellanic Cloud at 2.30 GHz J/A+AS/120/77 J/A+AS/120/77 Radio continuum study of the MC A radio continuum study of the Magellanic Clouds. Part IVa: Catalogues of radio sources in the Large Magellanic Cloud at 2.30 GHz M D Filipovic G L White R F Haynes P A Jones D Meinert R Wielebinski U Klein Astron. Astrophys. Suppl. Ser. 120 77 1996 1996A&AS..120...77F Magellanic Clouds Radio sources catalogs Magellanic Clouds radio continuum: galaxies We present a new catalogue of radio sources in the Large Magellanic Cloud (LMC) based on observations at 2.30GHz with the Parkes radio telescope. A total of 119 sources have been detected. We compare positions and flux densities of these sources with previously published radio results and find no significant positional displacement or flux discrepancies.
Catalogue of LMC sources at 2.30 GHz Source Source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin Des Declination (1950) arcsec SType Source type: when 'e' source is significantly extended --- FDens Flux density Jy Source cross-reference Number Source number --- Source Source name --- Comments Other names and comments number=1 N: Henize (1956ApJS....2..315H) MC: McGee et al. (1972AuJPh..25..613M) & (1972AuJPh..25..581M) MC4: Clarke et al. (1976AuJPS..40....1C) DEM: Davies et al. (1976MmRAS..81...89D) LHG: Long et al. (1981ApJ...248..925L) W: Wang et al. (1991ApJ...374..475W) NGC: Sinnot (1988, NGC 2000, Cambridge University Press, 46) PMN: Wright et al. (1994ApJS...91..111W) PSR: Taylor et al. (1993ApJS...88..529T) LH: Lucke et Hodge (1970AJ.....75..171L) Sa: Sanduleak et al. (1978PASP...90..621S) and Sanduleak (1984IAUS..108..231S) CO: Cohen et al. (1988ApJ...331L..95C) PKS: Otrupcek & Wright (1991, Proc. Astron. Soc. Australia 9, 170) IJL: Israel et al. (1993A&A...276...25I) RASS: Pietsch et al. (1996, A&A, in prep.) --- Patricia Bauer CDS 1996 Apr 22 J_A+AS_120_77.xml A 15 years monitoring program at 408 MHz J/A+AS/120/89 J/A+AS/120/89 408MHz observations A 15 years monitoring program at 408 MHz M Bondi L Padrielli R Fanti A Ficarra L Gregorini F Mantovani Astron. Astrophys. Suppl. Ser. 120 89 1996 1996A&AS..120...89B Galaxies, radio galaxies: active quasars: general radio continuum: galaxies This is the second paper based on the 408MHz monitoring program with the East-West arm of the Bologna interferometer. The monitoring concerned 125 radio sources measured approximately once a month for 15 years. We present the summary of the variability analysis concerning all the sample and the monitoring data, not yet published, of the variable sources.
Calibrator sources IAU IAU name --- Name Other name when available --- <F> Average flux density at 408 MHz Jy e_<F> rms scatter of the flux density Jy o_<F> Number of measurements --- Summary of monitored sources IAU IAU Name --- Name Other name when available --- Opt Optical identification --- z Redshift --- <F> Average flux density at 408MHz Jy e_<F> Scatter of variability deconvolved from experimental errors (only for variable and probably variable sources) Jy 2_<F> Normalized chi-squared --- o_<F> Number of observations --- Epoch1 First epoch of observation yr Epoch2 Last epoch of observation yr Var Code of variability (P = probably variable; V = variable) --- 408 MHz monitoring data of the variable and probable sources (table3 to table63) IAU IAU Name --- Name Other Name if available --- ObsDate Epoch of observation (dd mm yyyy) --- o_F Number of observations --- F Flux density at 408MHz Jy e_F Error on the flux density Jy Scint Percentage of scintillation % Note When -, the measurement is too affected by scintillation and not used in the statistical analysis --- Patricia Bauer CDS 1996 May 29 J_A+AS_120_89.xml Near infrared low-resolution spectra of 7 Be stars and AG Carinae J/A+AS/121/113 J/A+AS/121/113 Near-IR spectra of 7 Be stars and AG Car Near infrared low-resolution spectra of 7 Be stars and AG Carinae R E Mennickent C Sterken Astron. Astrophys. Suppl. Ser. 121 113 1997 1997A&AS..121..113M Equivalent widths Spectra, infrared Stars, Be stars: emission-line, Be stars: oscillations stars: variables: general We present and discuss {lambda} 6470-8780 spectra of 7 poorly-studied Be stars and of one Luminous Blue Variable (AG Car), and give equivalent widths and radial velocities of selected spectral lines.
HD 90966 10 28 18.4 -63 09 53 HD 91188 10 30 22.5 -57 04 38 HD 94366 10 53 01.2 -35 29 20 HD 94910 AG Car 10 56 11.6 -60 27 13 HD 124834 14 19 57.5 -73 58 05 HD 128293 14 39 31.7 -68 12 12 HD 179419 19 17 00.5 -65 13 39 HD 203699 21 23 35.2 +14 03 01
Normalized spectra lambda Wavelength 0.1nm F90966 HD 90966 normalized flux at lambda --- F91188 HD 91188 normalized flux at lambda --- F94366 HD 94366 normalized flux at lambda --- F94910 HD 94910 normalized flux at lambda --- F124834 HD 124834 normalized flux at lambda --- F128293 HD 128293 normalized flux at lambda --- F179419 HD 179419 normalized flux at lambda --- F203699 HD 203699 normalized flux at lambda --- Patricia Bauer CDS 1996 Dec 11 C. Sterken <csterken@vub.ac.be> J_A+AS_121_113.xml Optical photometric monitoring of gamma-ray loud blazars. I. Observations from November 1994 to November 1995. J/A+AS/121/119 J/A+AS/121/119 Optical monitoring of gamma-ray loud blazars. I Optical photometric monitoring of gamma-ray loud blazars. I. Observations from November 1994 to November 1995. M Villata C M Raiteri G Ghisellini G De Francesco S Bosio G Latini B Bucciarelli M Chiaberge G Chiumiento A Cora L Lanteri M G Lattanzi G Massone A Peila F Racioppi R L Smart F Scaltriti E Anderlucci Astron. Astrophys. Suppl. Ser. 121 119 1997 1997A&AS..121..119V Magnitudes QSOs gamma rays: theory quasars: general The results of the optical monitoring between November 1994 and November 1995 of twenty gamma-ray loud blazars included in the Torino blazar monitoring program are presented.
Photometric sequences for some of the monitored blazars Name Blazar designation --- Star Star designation --- Rmag R magnitude mag Vmag V magnitude mag Bmag B magnitude mag Sparse observations in the V band Name Blazar designation --- Date Observation date "DD/MM/YY" HJD Heliocentric Julian date d Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag *BVR observations Name Blazar designation --- Date Observation date "DD/MM/YY" HJD Heliocentric Julian date d n_Bmag D indicates that Bmag contains B-Bmin value --- Bmag B magnitude mag e_Bmag rms uncertainty on B magnitude mag n_Vmag D indicates that Vmag contains V-Vmin value --- Vmag V magnitude mag e_Vmag rms uncertainty on V magnitude mag n_Rmag D indicates that Rmag contains R-Rmin value --- Rmag R magnitude mag e_Rmag rms uncertainty on R magnitude mag UBVRI photopolarimetric observations of 2254+074 Source Source name --- Date Observation date "DD/MM/YY" HJD Heliocentric Julian date d Umag U magnitude mag e_Umag rms uncertainty on Umag mag PUmag Polarisation in U band % e_PUmag rms uncertainty on PU % PAUmag Position angle in U band deg e_PAUmag rms uncertainty on PAUmag deg Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag PBmag Polarisation in B band % e_PBmag rms uncertainty on PBmag % PABmag Position angle in B band deg e_PABmag rms uncertainty on PABmag deg Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag PVmag Polarisation in V band % e_PVmag rms uncertainty on PVmag % PAVmag Position angle in V band deg e_PAVmag rms uncertainty on PAVmag deg Rmag R magnitude mag e_Rmag rms uncertainty on Rmag mag PRmag Polarisation in R band % e_PRmag rms uncertainty on PRmag % PARmag Position angle in R band deg e_PARmag rms uncertainty on PARmag deg Imag I magnitude mag e_Imag rms uncertainty on Imag mag PImag Polarisation in I band % e_PImag rms uncertainty on PImag % PAImag Position angle in I band deg e_PAImag rms uncertainty on PAImag deg tables.tex TeX version of the tables fig9.ps Finding chart of OJ 248 fig11.ps Finding chart of 4C 71.07 fig13.ps Finding chart of 3C 216 fig20.ps Finding chart of PKS 1229-021 fig23.ps Finding chart of 3C 279 fig26.ps Finding chart of PKS 1510-089 fig27.ps Finding chart of DA 406 fig33.ps Finding chart of 4C 38.41 Patricia Bauer CDS 1996 Jun 03 M. Villata <villata@otoax3.to.astro.it> J_A+AS_121_119.xml Spectroscopy of the open cluster Blanco 1. II. Halpha emission as an indicator of relative age J/A+AS/121/213 J/A+AS/121/213 BV photometry of Blanco 1 stars Spectroscopy of the open cluster Blanco 1. II. Halpha emission as an indicator of relative age P M Panagi M A O'Dell Astron. Astrophys. Suppl. Ser. 121 213 1997 1997A&AS..121..213P Clusters, open Photometry open clusters and associations: individual (Blanco 1) stars: activity stars: chromospeheres stars: late-type We present the results of H{alpha}(6562A) and Li I(6708A) observations of 114 low-mass stars of the young open cluster Blanco 1. We also present observations of 30 stars in Ca II(K). This work extends the first Blanco 1 spectroscopic study of Panagi et al. (1994A&A...285..233D). From a sample of four well-studied clusters, including Blanco 1, we find that the fraction of H{alpha} emission-line stars amongst K dwarfs is a good indicator of relative age, with a smaller fraction indicative of older age. Blanco 1 shows a relatively small fraction of emitters, inconsistent with previous age estimates for the cluster. We estimate the cluster age to to be 90+/-25Myr, slightly older than the Pleiades. The method is shown to be more sensitive to age than lithium and a useful alternative to other age measurement techniques. The variation of H{alpha} with (B-V) is similar to that observed in the older solar neighbourhood dwarfs, suggesting that, at least for the absorption-line stars, the contribution of stellar rotation to the equivalent width is unclear. We combine both spectroscopy and photometry to revise cluster membership and give accurate positions for all these stars.
Blanco 1 C 0001-302 zeta Scl cluster 00 04.3 -29 56
APM positions of proposed members of the open-cluster Blanco 1. ZS ZS number (de Epstein & Epstein (1985)) --- m_ZS Multyiplicity index on ZS --- n_ZS Note on ZS number=1 ** = binary + = possible error in position. # = close pair/group, target in doubt or unresolved by the APM. ~ = not recovered by the APM. --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Vmag V magnitude mag B-V B-V color index mag Name Other designations number=2 W = Star No. assigned by Westerlund et al. (1988, <J/A+AS/76/101>) E = Star No. assigned by Epstein (1968AJ.....73..556E) HD = Henry Draper Catalogue number --- Positions of stars/objects classified as non-members. ZS ZS number (de Epstein & Epstein, 1985) --- West Westerlund number (Westerlund et al. (1988)) --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Vmag V magnitude mag B-V B-V color index mag Rem Remarks number=1 The publication/source where non-membership status was first given, P78 = Perry, Walter & Crawford (1978PASP...90...81P) A85 = Abraham de Epstein & Epstein (1985AJ.....90.1211D) W88 = Westerlund et al (1988A&AS...76..101W, Cat. <J/A+AS/76/101>) P94 = Panagi et al (1994A&A...285..233D) P96 = this paper. and criterion, where: pm = proper motion studies. ph = photometry. sp = spectroscopy. ns = non-stellar object --- Patricia Bauer CDS 1996 Jun 03 J_A+AS_121_213.xml GPM1 - a catalog of absolute proper motions of stars with respect to galaxies J/A+AS/121/243 J/A+AS/121/243 GPM1 catalogue GPM1 - a catalog of absolute proper motions of stars with respect to galaxies S P Rybka A I Yatsenko Astron. Astrophys. Suppl. Ser. 121 243 1997 1997A&AS..121..243R I/196 : HIPPARCOS Input Catalogue (HIC) V/131 : SAO Star Catalog J2000 (SAO) Proper motions astrometry reference systems GPM1 is the first version of the General Compiled Catalogue of Absolute Proper Motions for a sample of HIPPARCOS stars, derived with respect to galaxies within the plan called Catalogue of Faint Stars (KSZ, Deutch A.N., 1952IAUT....8..789D). The programme was proposed for several observatories of the former Soviet Union, China, Rumania and Spain. There are some resulting individual catalogues of absolute proper motions of stars compiled at five observatories (Kiev, Pulkovo, Moscow, Tashkent and Shanghai). The principal aim of the GPM1 construction was to provide absolute proper motions of stars to determine the rotation of the HIPPARCOS system. The GPM1 catalogue comprises absolute proper motions for 977 stars in 180 areas north of -25 degrees of declination. The mean square error is 8mas/yr on average. The standard errors differ from one star to another one depending on the number and quality of individual catalogues. They have been computed and presented for each star. For a single GPM1 field the absolute zero-point error of linking proper motions to the galaxies is 3mas/yr on average. The error of such a kind depends on the number and compactness of the galaxies available in each field. In addition to absolute proper motions and their mean errors, the catalogue gives the following data for each star: right ascension, declination, epoch for position, V-magnitude and number, copied from HIC. The stars were also identified with the objects of the Smithsonian Astrophysical Observatory Star Catalogue (SAO) list. Positions are given for equator and equinox J2000.0 on the system of FK5. They were presented to identify the GPM1 stars with those from other catalogues. The data file is sorted by J2000.0 right ascensions.
The GPM1 catalogue GPM1 GPM1 running number. --- No Region number number=1 Numbers from 1 to 205 are given according to the KSZ plan, numbers larger than 205 are NGC numbers of centre galaxies. --- HIC HIPPARCOS Input Catalogue (HIC) number (Catalogue <I/196>) --- Vmag V magnitude, copied from HIC. mag RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Epoch-1900 The epoch for the position. number=2 The epoch for the position: blank for J2000.0; otherwise (Epoch-1900), copied from HIC. yr pmRA Absolute proper motion in RA, multiplied by cos(Dec) mas/yr pmDE Absolute proper motion in Dec. mas/yr e_pm Mean error of proper motion. mas/yr SAO SAO Catalogue number (Catalogue <V/131>) --- Patricia Bauer CDS 1996 May 06 Svetlana P. Rybka <rybka@mao.gluk.apc.org> J_A+AS_121_243.xml UBV photometry of galactic foreground and LMC member stars. II. Galactic foreground stars (supplement) J/A+AS/121/247 J/A+AS/121/247 LMC galactic foreground stars UBV photometry UBV photometry of galactic foreground and LMC member stars. II. Galactic foreground stars (supplement) H -G Grothues M O Oestreicher J Gochermann C Tappert A Zaum H R Brugger T Schmidt-Kaler Astron. Astrophys. Suppl. Ser. 121 247 1997 1997A&AS..121..247G J/A+AS/99/591 : UBV Photometry of Galactic Foreground and LMC Member Stars Ardeberg A., Brunet J.P., Maurice E., Prevot L. 1972, A&AS 6, 249 =1972A&AS....6..249A Brunet J.P., Imbert M., Martin N., Mianes P., Prevot L., Rebeirot E., Rousseau J. 1975, A&AS 21, 109 =1975A&AS...21..109B Feast M.W., Thackeray A.D., Wesselink A.J. 1960, MNRAS 124, 337 =1960MNRAS.121..337F Feast M.W., Catchpole R.M., Carter B.S., Roberts G. 1980, MNRAS 193, 377 =1980MNRAS.193..377F Fehrenbach Ch., Duflot M. 1970, A&ASS 1, 1 =1970A&ASS...1....1F Fehrenbach Ch., Duflot M. 1973, A&AS 10, 231 =1973A&AS...10..231F Fehrenbach Ch., Duflot M. 1982, A&AS 48, 409 =1982A&AS...48..409F Gochermann J., Grothues H.-G., Oestreicher M.O., Berghoefer Th., Schmidt-Kaler Th. 1993, A&AS 99, 591 =1993A&AS...99..591G Houk, N., Cowley, A.P. 1975, University of Michigan Catalogue of Two Dimensional Spectral Types for the HD Stars, Vol. 1, Dept. of Astronomy, University of Michigan, Ann Arbor =Cat. <III/31> Leavitt H.S. 1908, Harvard Ann. 60, 87 =1908AnHar..60...87L Lucke P.B. 1972, Ph.D. Thesis, University of Washington Lucke P.B., Hodge P.W. 1970, AJ 75, 171 =1970AJ.....75..171L Nicolet B. 1978, A&AS 34, 1 =1978A&AS...34....1N Perie J., Prevot L., Rousseau M., Peyrin Y., Robin A. 1991, A&AS, 90, 1 =1991A&AS...90....1P Rebeirot E., Martin N., Mianes P., Prevot L., Robin A., Rousseau J., Peyrin Y. 1983, A&AS 51, 277 =1983A&AS...51..277R Reid N., Tinney C., Mould J. 1990, ApJ 348, 98 =1990ApJ...348...98R Sanduleak N. 1969, CTIO Contributions, no. 89 Sanduleak N., Philip A.G.D. 1977, Publ. of the Warner and Swasey Obs. 5, no.2 =1977PW&SO...2..105S Stock J., Osborn W., Ibanez M. 1976, A&AS 24, 35 =1976A&AS...24...35S Westerlund B.E., Olander N., Hedin B. 1981, A&AS 43, 267 =1981A&AS...43..267W Magellanic Clouds Photometry, UBV catalogs Galaxy: stellar content Magellanic Clouds In addition to the list of UBV photometries of 955 galactic foreground stars in the direction to the Large Magellanic Cloud published by Gochermann et al. (1993A&AS...99..591G), a supplement of 545 stars is presented, which have been measured with the same photometric accuracy. Moreover, less reliable photometries of 379 further foreground stars are listed in a separate table. The homogeneous data base of more than 1500 high accuracy photometries represented by these stars has been used to construct a reddening distribution map of the galactic foreground towards the LMC by Oestreicher et al. (1995A&AS..112..495O).
UBV photometries of LMC galactic foreground stars (at least 2 measurements, and quality 2 for V and B-V) UBV photometries of LMC galactic foreground stars (only 1 measurement, or quality 1 for V or B-V) HD HD/HDE number --- Name Other identifiers given in catalogues of LMC foreground and member stars, as well as in the Harvard Variable list number=1 A : Ardeberg (1972A&AS....6..249A) B : Brunet et al. (1975A&AS...21..109B) FD : Fehrenbach & Duflot (1970A&ASS...1....1F, 1973A&AS...10..231F, and 1982A&AS...48..409F) G : foreground stars erroneously identified as LMC members by Fehrenbach & Duflot (1970A&ASS...1....1F) GSC : HST Guide Star Catalogue HV : Harvard Variable, Leavitt (1908AnHar..60...87L) LH : Lucke & Hodge (1970AJ.....75..171L), Lucke (1972Thesi.........L) NS : Sanduleak (1969, CTIO Contributions, no. 89) RM : Rebeirot et al. (1983A&AS...51..277R) RV : Feast et al. (1960MNRAS.121..337F) S : Fehrenbach & Duflot (1970A&ASS...1....1F) SP : Sanduleak & Philip (1977PW&SO...2..105S) STO : Stock et al. (1976A&AS...24...35S) TRM : Reid et al. (1990ApJ...348...98R) WOH : Westerlund et al. (1981A&AS...43..267W) WOHg: Westerlund et al. (1981A&AS...43..267W), LMC giants --- o_Vmag Number of measurements --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V color index mag e_B-V rms uncertainty on B-V mag U-B U-B color index mag e_U-B rms uncertainty on U-B mag q_Vmag Quality of V as defined by Nicolet (1978A&AS...34....1N) --- q_B-V Quality of B-V as defined by Nicolet (1978A&AS...34....1N) --- q_U-B Quality of U-B as defined by Nicolet (1978A&AS...34....1N) --- Rem An asterisk indicates a remark, a number refers to the identification charts of Fig.3 number=2 Remarks to Table 2: HD 29921 double star (Perie et al. 1991A&AS...90....1P) HD 33487 variable ? HD 33986 double star (dist. = 10") HD 34397 double star HD 34650 double star (dist. = 9") HD 34871 double star HD 36347 double star (Perie et al. 1991A&AS...90....1P); UBV measured for brighter component A HD 36584 double star (dist. = 2") HD 36818 double star HD 37262 double star (Perie et al. 1991A&AS...90....1P); UBV measured for brighter component A HD 37298 variable ?; M5-7: III (Houk & Cowley 1975, Cat. <III/31>) HD 38329 double star HDE 268776 already published in Paper I (2 measurements) HDE 269072 double star HDE 269104 double star (dist. = 10") HDE 269266 double star (dist. = 3") HDE 269268 double star HDE 269368 HV 5748, but no variability detected HDE 269521 spectroscopic binary (Ardeberg et al. 1972A&AS....6..249A) HDE 269532 double star (dist. = 11") HDE 269632 double star (dist. = 10") HDE 269894 double star (dist. = 3") HDE 270001 double star ? HDE 270097 double star HDE 270104 double star (dist. = 11") HDE 270135 variable ? HDE 270207 variable ? HDE 270277 double star (dist. = 10") HDE 270336 double star (dist. = 9") HDE 270382 double star (dist. = 14") HDE 271058 double star (dist. = 8") FD 324 variable ? FD 427 double star (dist. = 7") FD 460 variable ? FD 579 double star (dist. = 11") FD 1714 variable ? FD 2056 double star (dist. = 6") FD 2072 double star (dist. = 2") FD 2588 double star (dist. = 6") Remarks to Table 3: HD 32229 variable ? HDE 268823 NGC 1786 (Fehrenbach & Duflot 1982A&AS...48..409F); erroneously designated as FD 428 by Fehrenbach & Duflot (1982A&AS...48..409F) HDE 268839 double star (dist. = 10") HDE 268855 double star (dist. = 13"); variable ? HDE 268906 double star (dist. = 12") HDE 269453 variable ? HDE 269960 variable ? HDE 270028 double star (dist. = 13") HDE 270166 double star (dist. = 5") HDE 270666 double star (dist. = 6"); both components measured in common (A = FD 105, B = FD 106, cf. FD 106) HDE 270688 variable ? HDE 271062 double star (dist. = 12") HDE 271517 double star (dist. = 2.7", Ardeberg et al. 1972A&AS....6..249A) GSC 9163 729 variable ? GSC 9166 291 variable ? FD 55 double star ? FD 106 cf. HDE 270666 FD 666 variable ? FD 867 variable ? FD 1769 variable ? FD 2741 double star ? FD 2839 double star (dist. = 10") HDE 268910F identical with FD 442 = HD 32779 (cf. Gochermann et al. 1993A&AS...99..591G) TRM 40 variable ? WOHg 22 late type M III (Westerlund et al. 1981A&AS...43..267W) WOHg 61 variable ?; late type M III (Westerlund et al. 1981A&AS...43..267W) WOHg 130 variable with period of 335 days (Feast et al. 1980MNRAS.193..377F); late type M III (Westerlund et al. 1981A&AS...43..267W) --- Patricia Bauer CDS 1996 May 21 Hans-Georg Grothues <hgg@astro.ruhr-uni-bochum.de> J_A+AS_121_247.xml A radio continuum study of the Magellanic Clouds. Part V: Catalogues of radio sources in the Small Magellanic Cloud at 1.42, 2.45, 4.75, 4.85 and 8.55 GHz. J/A+AS/121/321 J/A+AS/121/321 SMC catalogue of radiosources A radio continuum study of the Magellanic Clouds. Part V: Catalogues of radio sources in the Small Magellanic Cloud at 1.42, 2.45, 4.75, 4.85 and 8.55 GHz. M D Filipovic P A Jones G L White R F Haynes U Klein R Wielebinski Astron. Astrophys. Suppl. Ser. 121 321 1997 1997A&AS..121..321F VIII/15 : The Parkes Radio Sources Catalogue (PKSCAT90) (Wright+ 1990) J/A+AS/111/311 : Part IV: LMC radiosources at 1.40, 2.45, 4.75, 4.85 & 8.55GHz Bruhweiler F.C. et al., 1987, ApJ 317, 152 =1987ApJ...317..152B Clarke J.N. et al., 1976, Aust. J. Phys. Supp. 40, 1 =1976AuJPS..40....1C Davies R.D. et al., 1976, Mem. R. Astron. Soc. 81, 89 =1976MmRAS..81...89D Filipovic M.D. et al., Part IV, 1995, A&AS, 111, 311 =Cat <J/A+AS/111/311> Haynes R.F. et al., Part I, 1986, A&A, 159, 22 =1986A&A...159...22H Henize K.G., 1956 ApJS 2, 315 =1956ApJS....2..315H Inoue et al. 1983, IAUS 101, 535 =1983IAUS..101..535I Israel F.P. et al., 1993, A&A 276, 25 =Cat <J/A+A/276/25> Klein U. et al., Part II, 1989, A&A, 211, 280 =1989A&A...211..280K Large M.I. et al., 1981, MNRAS 194, 693 =Cat <VIII/16> McGee R.X. et al., 1976, Aust. J. Phys. 29, 329 =1976AuJPh..29..329M Mills B.Y. & Aller L.H., 1971, Aust. J. Phys. 24, 609 =1971AuJPh..24..609M Otrupcek R.E. & Wright A.E., 1991, Proc. Astron. Soc. Australia 9, 170 =1991PASAu...9..170O Seward F.D. & Mitchell M., 1981, ApJ 243, 736 =1981ApJ...243..736S Sinnott R.W., NGC 2000, 1988, Cambridge Univ. Press, 46 Wang Q. & Wu X., 1992, ApJS 78, 391 =1992ApJS...78..391W Wright G.L. et al., 1994, APJS 91,111 =1994ApJS...91..111W Xu C. et al., Part III, 1992, A&A, 257, 47 =1992A&A...257...47X Magellanic Clouds Positional data Radio sources catalogs Magellanic Clouds radio continuum: galaxies radio continuum: general We present catalogues of radio sources in the Small Magellanic Cloud from observations with the Parkes radio telescope at 1.42, 2.45, 4.75 and 8.55GHz, and an additional catalogue from the Parkes-MIT-NRAO survey at 4.85GHz. A total of 224 sources were detected at at least one of these frequencies, 60 of which are reported here for the first time as radio sources. We compare positions and flux densities of these sources with previously published results and find no significant positional displacement or flux discrepancies.
Catalogue of SMC Sources at 1.42 GHz Catalogue of SMC Sources at 2.45 GHz Catalogue of SMC Sources at 4.75 GHz Catalogue of SMC Sources at 4.85 GHz Catalogue of SMC Sources at 8.55 GHz Name SMC name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec e Extension flag (see Note (1) for radio) --- FD Flux density Jy SMC Sources (Tables 2-6 as a single table) Name SMC name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec e Extension flag number=1 The definition adopted here for a significantly extended source is that the fitted size (solid angle) of the source is twice that of the effective beam size. The true angular size of the sources is the observed size deconvolved with the effective beam size. This means that for circular sources the deconvolved diameter of an 'extended' source is greater than the effective beam size. The effective beam sizes are in Table 1: Frequency Effective beam size (GHz) (arcmin) ------------------------------- 1.42 16.8 2.45 10.1 4.75 5.3 4.85 5.2 8.55 3.6 --- Freq Frequency GHz S(Freq) Flux density at Freq Jy Source Cross-reference No Sequence number --- Name SMC name ( Small Magellanic Cloud, B1950) --- Names Other designations number=1 the following designations are used: N : Henize (1956ApJS....2..315H) (e.g., N 66) S : McGee et al. (1976AuJPh..29..329M) (e.g., S 17) PKS : Otrupcek & Wright (1991PASAu...9..170O) (e.g. PKS B0057-724) MC4 : Clarke et al. (1976AuJPS..40....1C) (e.g., MC4 B0057-724) MRC : Large et al. (1981MNRAS.194..693L) (e.g., MRC B0027-698) MA : Mills & Aller (1971AuJPh..24..609M) (e.g., MA B0103-723) PMN : Wright et al. (1994ApJS...91..111W) (e.g., PMN J0059-7210) NGC : Sinnott (1988, Cambridge Univ. Press, 46) (e.g., NGC 346) DEM : Davies et al. (1976MmRAS..81...89D) (e.g., DEM 103) 1E : Seward & Mitchell (1981ApJ...243..736S) (e.g., 1E0057.6-7228) IKT : Inoue et al. (1983IAUS..101..535I) (e.g., IKT 18) LI-SMC : Israel et al. (1993A&A...276...25I) (e.g., LI-SMC 131) WW : Wang & Wu (1992ApJS...78..391W) (e.g., WW 44) BKGS : Bruhweiler et al. (1987ApJ...317..152B) (e.g. BKGS 1A) --- Patricia Bauer CDS 1996 Jun 18 Paul Jones <P.Jones@st.nepean.uws.edu.au> UNKNOWN UNKNOWN Corrections in table7 made the 30-Jun-1997: For No. 208 , MRC B029-701 was transformed in MRC B0129-701, For No. 213 , MRC B032-697 was transformed in MRC B0132-697. J_A+AS_121_321.xml Nonlinear investigation of the pulsational properties of RR Lyrae variables J/A+AS/121/327 J/A+AS/121/327 RR Lyr pulsational model Nonlinear investigation of the pulsational properties of RR Lyrae variables G Bono F Caputo V Castellani M Marconi Astron. Astrophys. Suppl. Ser. 121 327 1997 1997A&AS..121..327B Effective temperatures Radial velocities Stars, variable globular clusters: individual (M 3, M 5, M 15) RR Lyrae variable stars: horizontal-branch stars: oscillations stars: variables: other We present a theoretical investigation on periods and amplitudes of RR Lyrae pulsators by adopting stellar parameters which cover the range of theoretical evolutionary expectations. Extensive grids of nonlinear, nonlocal and time-dependent convective RR Lyrae envelope models have been computed to investigate the pulsational behavior in both fundamental and first overtone modes at selected luminosity levels and over an effective temperature range which covers the whole instability region. In order to avoid spurious evaluations of modal stability and pulsation amplitudes, the coupling between pulsation and convection was followed through a direct time integration of the leading equations until radial motions approached their limiting amplitude. Blue and red boundaries for pulsational instability into the HR diagram are presented for three different mass values M=0.75, 0.65 and 0.58M_{sun}_, together with an atlas of full amplitude theoretical light curves for both fundamental and first overtone pulsators and for two different assumptions of stellar masses: M=0.75 and 0.65M_{sun}_.
Fundamental Nonlinear Survey for M=0.58M_{sun}_ First Overtone Nonlinear Survey for M=0.58M_{sun}_ Fundamental Nonlinear Survey for M=0.65M_{sun}_ First Overtone Nonlinear Survey for M=0.65M_{sun}_ Fundamental Nonlinear Survey for M=0.75M_{sun}_ First Overtone Nonlinear Survey for M=0.75M_{sun}_ logL Luminosity solLum Model Model number number=1 (-): pulsationally stable (+): pulsationally instable (#): mixed mode (mixture of different radial modes or amplitude modulations) (*): switch mode (fundamental toward first overtone or viceversa) --- Teff Static effective temperature K NP Number of period covered during the direct time integration --- P Non-linear period d DR/Rph Fractional radial oscillation (Rmax-Rmin)/Rph where Rph is the photospheric radius --- Du Radial velocity amplitude (u_max - u_min) km/s DMbol Bolometric amplitude (Mbol_max - Mbol_min) mag Dloggs Logarithmic amplitude of the static surface gravity (loggs_max - loggs_min) cm/s2 Dloggeff Logarithmic amplitude of the effective surface gravity (loggeff_max - loggeff_min) cm/s2 DT Surface temperature amplitude (T_max - T_min) K DTeff Surface effective temperature amplitude K appen.tex LaTeX version of Appendix table5.tex LaTeX version of table5 table6.tex LaTeX version of table6 table7.tex LaTeX version of table7 table8.tex LaTeX version of table8 table9.tex LaTeX version of table9 table10.tex LaTeX version of table10 Patricia Bauer CDS 1996 Jun 18 J_A+AS_121_327.xml Accurate positions and finding charts of known planetary nebulae in the Large Magellanic Cloud. J/A+AS/121/407 J/A+AS/121/407 LMC planetary nebulae positions Accurate positions and finding charts of known planetary nebulae in the Large Magellanic Cloud. P Leisy M Dennefeld C Alard J Guibert Astron. Astrophys. Suppl. Ser. 121 407 1997 1997A&AS..121..407L J/MNRAS/234/583 : Abundances in Magellanic Cloud planetary nebulae J/ApJS/75/407 : PNe Magellanic Cloud optical spectroscopy. I J/ApJS/76/1085 : PNe Magellanic Cloud optical spectroscopy. II J/ApJS/83/87 : PNe Magellanic Cloud optical spectroscopy. III Magellanic Clouds Planetary nebulae astrometry galaxies: ISM galaxies: stellar content Magellanic Clouds planetary nebulae: general We present identifications and accurate positions for about 280 planetary nebulae (PNe) in the Large Magellanic Cloud (LMC). These positions are needed for follow-up ground or space observations. Entire Schmidt plates have been scanned with the MAMA micro-densitometer, and PPM stars used for the astrometric reduction. The precision achieved is always better than 0.5", and better than 0.3" for most of the objects not located close to the border of the plates. Photometry in the B band is provided with an accuracy of about 0.2magnitude, except in too crowded zones where the background cannot be determined. Cross-identifications with IRAS sources have also been tabulated and discussed.
277 PNe coordinates in the LMC Name Name --- OtherName Other name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec RAh1 Right ascension (B1950) h RAm1 Right ascension (B1950) min RAs1 Right ascension (B1950) s DE-1 Declination sign --- DEd1 Declination (B1950) deg DEm1 Declination (B1950) arcmin DEs1 Declination (B1950) arcsec Flag Position Error Flag --- Ntot Total number of frames on which a position has been measured --- Neff Number of frames effectively used --- Bmag Magnitude in B filter mag o_Bmag Number of frames used for the magnitude determination --- Patricia Bauer CDS 1996 Oct 03 Pierre Leisy <leisy@iap.fr> J_A+AS_121_407.xml CCD Photometry of distant open clusters: III. Berkeley 18. J/A+AS/121/455 J/A+AS/121/455 BVI photometry of stars in Berkeley 18 CCD Photometry of distant open clusters: III. Berkeley 18. J Kaluzny Astron. Astrophys. Suppl. Ser. 121 455 1997 1997A&AS..121..455K Clusters, open Photometry, CCD Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Berkeley 18) We present CCD BVI photometry for Berkeley 18, a rich open cluster located in the Galactic anticenter. The cluster age is similar to, or marginally lower than age of M 67. Its distance is estimated at 5.8kpc and the reddening E(B-V) is probably higher than 0.46. Our data indicate that Be 18 is one of the most populous objects in the whole sample of known galactic open clusters. The angular diameter of the cluster is estimated at 26arcmin, which corresponds to a linear size of about 44pc. The horizontal branch of Be 18 exhibits a large width in comparison with other old open clusters.
Berkeley 18 C 0518+453 05 22.2 +45 24
BV photometry of stars from Berkeley 18 field October 91, 2.1-m telescope data BV photometry of stars from Berkeley 18 field October 92, 2.1-m telescope data BV photometry of stars from Berkeley 18 field October 92, 0.9-m telescope data ID ID number --- Xpos X coordinate number=1 1 pixel=0.30 arcsec; X axis points toward North; Y axis points toward East pix Ypos Y coordinate number=1 1 pixel=0.30 arcsec; X axis points toward North; Y axis points toward East pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag o_Vmag number of averaged V measurements --- q_Vmag quality flag for Vmag number=2 q=1 means relatively poor quality --- B-V B-V color index mag e_B-V rms uncertainty on B-V number=3 blank means "unknown color" mag o_B-V Number of averaged B measurements --- q_B-V Quality flag for B-V --- V-I V-I color index mag e_V-I rms uncertainty on V-I number=3 blank means "unknown color" mag o_V-I Number of averaged I measurements --- q_V-I Quality flag for V-I --- Patricia Bauer CDS 1996 Jun 24 Janusz Kaluzny <jka@vela.astrouw.edu.pl> J_A+AS_121_455.xml Ultraviolet variability of the Seyfert 1 galaxy Fairall 9 J/A+AS/121/461 J/A+AS/121/461 UV variability of Fairall-9 Ultraviolet variability of the Seyfert 1 galaxy Fairall 9 M C Recondo-Gonzalez W Wamsteker J Clavel P M Rodriguez-Pascual R Vio T -G Wang M Santos-Lleo F Makino Astron. Astrophys. Suppl. Ser. 121 461 1997 1997A&AS..121..461R Galaxies, Seyfert Spectra, ultraviolet galaxies: individual (Fairall 9) galaxies: Seyfert ultraviolet: galaxies This is a study of the UV variability of the galaxy Fairall-9 between 1978 and 1991. Table 1 shows the UV continuum fluxes measured in three "line-free" windows centered at 1171, 1400 and 1910 A (observed wavelengths), and corrected for E(B-V)=0.035 extinction. The IUE Fine Error Sensor (FES) counts (optical photometry) are also given in this table, corrected for the same extinction. Tables 10, 11, 12 and 13 show the variability of the components for the main UV lines (Ly{alpha}+NV, SiIV, CIV and MgII). Line profile variability has been used to isolate four gaussian line components, which are sufficient to describe all lines at all levels of brightness in a consistent way: one narrow (i.e. unresolved at the IUE resolution) and three broad components: a central (velocity same as the narrow line), a redshifted (v=3300 km/s) and a blue shifted one (v=-3600 km/s). The Ly{alpha}-NV blend is fitted together in the Ly{alpha} region (Table 10), to account the NV presence (one narrow and one red component). The results for SiIV are shown in Table 11. In CIV (Table 12) have been included a very weak component bluer than the blue component, most likely associated with NIV] 1486. Table 13 shows MgII results.
Fairall 9 01 23 45.70 -58 48 21.6
UV-FES continuum fluxes corrected for E(B-V)=0.035 HJD Heliocentric Julian date d F1171 Continuum Flux at 1171A (1158-1184A) number=1 The wavelengths are the observed ones. Fluxes given in E-14*erg s-1 cm-2 A-1 10-16W/m2/nm e_F1171 rms uncertainty on Flux at 1171A 10-16W/m2/nm F1400 Continuum Flux at 1400A (1390-1410A) number=1 The wavelengths are the observed ones. Fluxes given in E-14*erg s-1 cm-2 A-1 10-16W/m2/nm e_F1400 rms uncertainty on Flux at 1400A 10-16W/m2/nm F1910 Continuum Flux at 1910A (1895-1925A) number=1 The wavelengths are the observed ones. Fluxes given in E-14*erg s-1 cm-2 A-1 10-16W/m2/nm e_F1910 rms uncertainty on Flux at 1910A 10-16W/m2/nm FES IUE Fine Error Sensor counts (optical) ct e_FES rms uncertainty on FES counts ct Ly{alpha}lambda 1216 and NV lambda 1240 components HJD Heliocentric Julian date d F1400 Continuum Flux at 1400 Angstroms number=1 Fluxes given in E-14*erg s-1 cm-2 A-1 10-16W/m2/nm e_F1400 rms uncertainty on Flux at 1400A 10-16W/m2/nm Narrow Ly{alpha} Narrow Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Narrow rms uncertainty on Narrow 10-17W/m2 Central Ly{alpha} Central Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Central rms uncertainty on Central 10-17W/m2 Red Ly{alpha} Red Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Red rms uncertainty on Red 10-17W/m2 Blue Ly{alpha} Blue Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Blue rms uncertainty on Blue 10-17W/m2 NVn NV Narrow Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_NVn rms uncertainty on NVn 10-17W/m2 NVr NV Red Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_NVr rms uncertainty on NVr 10-17W/m2 SiIV lambda 1397 components HJD Heliocentric Julian date d F1400 Continuum Flux at 1400 Angstroms number=1 Fluxes given in E-14*erg s-1 cm-2 A-1 10-16W/m2/nm e_F1400 rms uncertainty on Flux at 1400A 10-16W/m2/nm Narrow SiIV Narrow Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Narrow rms uncertainty on Narrow 10-17W/m2 Central SiIV Central Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Central rms uncertainty on Central 10-17W/m2 Red SiIV Red Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Red rms uncertainty on Red 10-17W/m2 Blue SiIV Blue Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Blue rms uncertainty on Blue 10-17W/m2 CIV lambda 1549 components HJD Heliocentric Julian date d F1400 Continuum Flux at 1400 Angstroms number=1 Fluxes given in E-14*erg s-1 cm-2 A-1 10-16W/m2/nm e_F1400 rms uncertainty on Flux at 1400A 10-16W/m2/nm Narrow CIV Narrow Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Narrow rms uncertainty on Narrow 10-17W/m2 Central CIV Central Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Central rms uncertainty on Central 10-17W/m2 Red CIV Red Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Red rms uncertainty on Red 10-17W/m2 Blue CIV Blue Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Blue rms uncertainty on Blue 10-17W/m2 Blue2 Another CIV Blue Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Blue2 rms uncertainty on Blue2 10-17W/m2 MgII lambda 2798 components HJD Heliocentric Julian date d F1400 Continuum Flux at 1400 Angstroms number=1 Fluxes given in E-14*erg s-1 cm-2 A-1 10-16W/m2/nm e_F1400 rms uncertainty on Flux at 1400A 10-16W/m2/nm Narrow MgII Narrow Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Narrow rms uncertainty on Narrow 10-17W/m2 Central MgII Central Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Central rms uncertainty on Central 10-17W/m2 Red MgII Red Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Red rms uncertainty on Red 10-17W/m2 Blue MgII Blue Component number=2 Component integrated fluxes given in E-14*erg s-1 cm-2 10-17W/m2 e_Blue rms uncertainty on Blue 10-17W/m2 tables.tex LaTeX version of the tables M.C. Recondo-Gonzalez ESA IUE Obs. Patricia Bauer CDS 1996 Jun 28 Carmen Recondo-Gonzalez <cr@v3600.vilspa.esa.es> J_A+AS_121_461.xml CCD photometry of the globular cluster Palomar 13 J/A+AS/121/499 J/A+AS/121/499 BV and rg photometry of Pal 13 CCD photometry of the globular cluster Palomar 13 J Borissova H Markov N Spassova Astron. Astrophys. Suppl. Ser. 121 499 1997 1997A&AS..121..499B Clusters, globular Photometry, CCD globular clusters: individual (Palomar 13) Hertzsprung-Russell (HR diagram) A new CCD photometry of the halo cluster Palomar 13 is used to construct a color-magnitude diagram in the Thuan-Gunn and the B, V photometric systems. The color-magnitude diagram of the cluster shows as already noted by Ortolani et al. (1985AJ.....90..473O) an extremely poor red horizontal branch and a very sparsely populated giant branch. Seven BSS candidates are identified in the field of Palomar 13. The age of the cluster determined by fitting with the isochrones of Proffitt & Vanden Berg (1991ApJS...77..473P) and Bergbusch & Vanden Berg (1992ApJS...81..163B) and by a differential comparison of the color-magnitude diagram with that of Pal 5 is 12+/-2Gyr.
Pal 13 C 2304+124 23 06.5 +12 44
B,V photometry of Pal 13 ID Identification number --- Xpos X position (1 pix = 0.30 arcsec) pix Ypos Y position (1 pix = 0.34 arcsec) pix Vmag V magnitude mag B-V B-V color index mag g,r photometry of Pal 13 ID Identification number --- Xpos X position (1 pix = 0.30 arcsec) pix Ypos Y position (1 pix = 0.34 arcsec) pix gmag g magnitude mag g-r g-r color index mag Patricia Bauer CDS 1996 Jun 28 J. Borissova <leonid@phys.uni-sofia.bg> J_A+AS_121_499.xml Near infrared surface photometry of late-type Virgo cluster galaxies J/A+AS/121/507 J/A+AS/121/507 Near-IR surface photometry of Virgo galaxies Near infrared surface photometry of late-type Virgo cluster galaxies A Boselli R Tuffs G Gavazzi H Hippelein D Pierini Astron. Astrophys. Suppl. Ser. 121 507 1997 1997A&AS..121..507B Galaxies, IR Photometry, surface galaxies: clusters: individual (Virgo cluster) galaxies: fundamental parameters galaxies: photometry infrared: galaxies The basic parameters of galaxies observed in this work: table 3: total H and K' magnitudes derived using circular apertures; table 5: photometric parameters derived along elliptical apertures
Basic parameters of galaxies VCC VCC name (=1985AJ.....90.1681B) --- n_VCC Note on VCC name number=1 An * indicates galaxies not included in the sample as defined in Sect. 2. --- NGC/IC NGC/IC name (Catalogue <VII/1>) --- UGC UGC name (Catalogue <VII/26>) --- RAh Right Ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Mtype Morphological type --- a Optical major diameter arcmin b Optical minor diameter arcmin Bmag B magnitude (total) mag Hmag H magnitude (total) mag K'mag K' magnitude (total) mag Photometric parameters VCC VCC name (=1985AJ.....90.1681B) --- Filt Adopted filter --- IntTime Integration time per position s a Number of frames per galaxy --- m Adopted mosaic --- Size Pixel size arcsec Qphot Photometric quality --- PA Position angle deg u_PA Uncertainty flag on PA --- 1-b/a Ellipticity --- u_1-b/a Uncertainty flag on 1-b/a --- Note A 't' indicates "troncated", no following values --- a21.5 Isophotal diameter at 21.5mag/arcsec^2^ arcsec m21.5 Integrated magnitude at a21.5 mag c31_215 Concentration index at a21.5 --- a22 Isophotal diameter at 22mag/arcsec^2^ arcsec m22 Integrated magnitude at a22 mag c31_22 Concentration index at a22 --- Differential H and K' band radial surface brightness profiles VCC VCC name (=1985AJ.....90.1681B) --- Filt Adopted filter --- Rad Radius on the major axis of the ellipse arcsec SuBr Surface brightness at the given radius mag/arcsec2 Patricia Bauer CDS 1996 Jul 23 Alessandro Boselli <BOSELLI@astrsp-mrs.fr> J_A+AS_121_507.xml Fourth supplement to the catalogue of observed periods of Ap stars J/A+AS/121/57 J/A+AS/121/57 Ap stars periodicity Fourth supplement to the catalogue of observed periods of Ap stars F A Catalano P Renson Astron. Astrophys. Suppl. Ser. 121 57 1997 1997A&AS..121...57C III/152 : Catalogue of observed periods of Ap stars (Catalano+ 1984) (An updated version is in preparation) Catalano & Renson, 1984, A&AS 55, 371 (Catalogue) =Catalogue <III/152> Catalano & Renson, 1988, A&AS 72, 1 (First suppl.) =1988A&AS...72....1C Catalano et al., 1991, A&AS 87, 59 (Second suppl.) =1991A&AS...87...59C Catalano et al., 1993, A&AS 98, 269 (Third suppl.) =1993A&AS...98..269C Stars, Ap catalogs stars: chemically peculiar stars: variables: other New data on the periods of Ap stars with references are presented (Table 1). 21 further stars are introduced for which a periodic variability has recently been discovered or for which it was known before but it was not reported in previous issues of this catalogue. For many stars also present in previous issues of the catalogue new determinations of the periods are given. Recently attributed variable star names are also quoted.
The fourth supplement to the catalogue of the periods of Ap stars n_HD A '+' indicates a note number=1 + indicates stars which appear for the first time ** indicates a new or modified note (see note 1) * indicates stars which have a note in the preceding version with no changes (Catalano et al. 1984, 1988, 1991, 1993) --- HD HD number number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- HR HR number number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- n_HR Note on HR number=1 + indicates stars which appear for the first time ** indicates a new or modified note (see note 1) * indicates stars which have a note in the preceding version with no changes (Catalano et al. 1984, 1988, 1991, 1993) --- Name Other name number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- Name2 Other name number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- Sp Spectral type number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- Per Period number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' d u_Per Uncertainty flag on Period number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- n_Per Remark when no periodicity number=2 ':' period uncertain '?' period doubtful --- nPer Notes on Period number=3 'l' for luminosity and/or colour variations 'm' for magnetic field variations 's' for variations of intensity of certain spectral lines 'v' for variations of wavelength of certain spectral lines --- Per1 Proposed periodicities (in days) and references number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- Per2 Proposed periodicities (in days) and references number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- Per3 Proposed periodicities (in days) and references number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- Per4 Proposed periodicities (in days) and references number= [HD 36485]: ADS 4134C: the brighter component HD 36486 ({delta} Ori A = HR 1852, V = 2.23) 52" away, and a fainter component (ADS 4134B, V = 14) 33" away from A, are not physically related to HD 36485; HD 36485 is also a spectroscopic binary with P = 9.9144+/-0.0002d (Morrell & Levato 1991) [HD 37017]: sp. bin. P = 18.6217+/-0.0004 d (Morrell & Levato 1991) [HD 37479]: first helium-strong star in which a large magnetic field has been detected. Light variations are mainly due to the eclipse by a ring or cloud of circumstellar material (Groote & Hunger 1982) [HD 47152]: interf. bin. P = 25.8 years (Baize 1989) [HD 84041]: rapid oscillating Ap star with periods near 15 min; also visual double: fainter component (V = 13) at 8" [HD 116458]: sp. bin. P = 126 d [HD 143654]: according to the quoted authors, this star is probably not an Ap star [HD 144667]: component A (V = 6.64) of a quadruple system; companion B (V~13) at 16"; companion C (HD 144668 = HR 5999 = V856 Sco, irregular variable, Sp. A7IIIe, V ~ 7.0) at 44"; companion D (V ~ 11.6) at 1.3" from C [HD 165474]: ADS 11056B, component A at 7", {DELTA}m = 0.5; component C at 56" is 5 mag. fainter than A [HD 171247]: ADS 11448A, companion at 38.7", {DELTA}m = 4 [HD 180583]: this star is probably not to be considered as an Ap star, but it is a known cepheid, as it has been noted in the General Catalogue of Ap and Am Stars, its luminosity class being I or II [HD 191495]: star of the open cluster NGC 6871, in the association Cyg OB3 [HDE 335238]: (= Rns 55280): coordinates at the epoch 1950.0: 20^h^ 48.6^m^ +29^o^ 37' [Gr.9-NGC 2169]: (= Rns 11180): star N.9 in NGC 2169 (Grubissich 1959); the identification as star N.12 in Hoag et al. (1961) has also been used. Coordinates at the epoch 1950.0: 06h 05.6m, +13deg57' --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1996 May 28 F. Catalano <FCATALANO@alpha4.ct.astro.it> J_A+AS_121_57.xml CCD astrometry of Saturn's satellites 1990-1994 J/A+AS/121/65 J/A+AS/121/65 1990-1994 Saturn's satellites astrometry CCD astrometry of Saturn's satellites 1990-1994 D Harper C D Murray K Beurle I P Williams D H P Jones D B Taylor S C Greaves Astron. Astrophys. Suppl. Ser. 121 65 1997 1997A&AS..121...65H Planets Positional data satellites of Saturn astrometry In this paper, we publish 1206 measurements of positions of the major satellites of Saturn made in 1990, 1991, 1993 and 1994 using CCD detectors attached to the 1-metre Jacobus Kapteyn Telescope on the island of La Palma. Analysis of the data as inter-satellite positions shows that the observations of Tethys, Dione, Rhea and Titan have root-mean-square residuals of 0.08 arcseconds, corresponding to 500km at the distance of Saturn.
Observations made in 1990 Observations made in 1991 Observations made in 1993 Observations made in 1994 OBSy Year of the observation number=1 The year, month and day give U.T.C. time of the start of the exposure yr OBSmo Month of the observation number=1 The year, month and day give U.T.C. time of the start of the exposure "month" OBSd Day of the observation number=1 The year, month and day give U.T.C. time of the start of the exposure d Exp Length of the exposure; add half of this value to the start date to obtain the mid-exposure time s Boo Boolean flags indicating presence (1) or absence (0) of each satellite in the image --- xiMimas Column coordinate xi of Mimas, if present pix etaMimas Row coordinate eta of Mimas, if present pix xiEnc Column coordinate xi of Enceladus, if present pix etaEnc Row coordinate eta of Enceladus, if present pix xiTethys Column coordinate xi of Tethys, if present pix etaTethys Row coordinate eta of Tethys, if present pix xiDione Column coordinate xi of Dione, if present pix etaDione Row coordinate eta of Dione, if present pix xiRhea Column coordinate xi of Rhea, if present pix etaRhea Row coordinate eta of Rhea, if present pix xiTitan Column coordinate xi of Titan, if present pix etaTitan Row coordinate eta of Titan, if present pix xiHyp Column coordinate xi of Hyperion, if present pix etaHyp Row coordinate eta of Hyperion, if present pix xiIap Column coordinate xi of Iapetus, if present pix etaIap Row coordinate eta of Iapetus, if present pix Patricia Bauer CDS 1996 Jul 29 David Harper <D.Harper@qmw.ac.uk> J_A+AS_121_65.xml Orbits of new spectroscopic components in 7 multiple systems. J/A+AS/121/71 J/A+AS/121/71 Orbits of 7 spectroscopic binaries in multiples Orbits of new spectroscopic components in 7 multiple systems. A A Tokovinin Astron. Astrophys. Suppl. Ser. 121 71 1997 1997A&AS..121...71T Binaries, spectroscopic Radial velocities binaries: spectroscopic binaries: visual Individual radial velocities (heliocentric date, velocity, error) and residuals to orbits are given for components of 7 wide physical multiple systems.
ADS 1315 A 01 40 51.7 +49 52 55 ADS 1315 B 01 40 51.7 +49 52 55 ADS 1315 C 01 40 51.1 +49 52 56 ADS 1849 A 02 26 00.40 -15 20 26 ADS 1849 B 02 25 59.5 -15 20 19 ADS 1849 C 02 26 03.9 -15 18 51 ADS 1849 AB 02 25 59.8 -15 20 21 ADS 3608 A 05 01.7 +26 40 ADS 3608 B 05 01.7 +26 40 ADS 3608 C 05 01 46.29 +26 39 01 ADS 3608 AB 05 01 44.23 +26 40 14 ADS 3824 A 05 15 24.43 +32 41 15 ADS 3824 B 05 15 24.2 +32 41 25 ADS 3824 C 05 15 23.55 +32 41 06 ADS 3824 D 05 15 15.3 +32 43 37 ADS 3824 ABC 05 15 23.9 +32 41 15 ADS 3991 AxBC 05 23.9 -00 53 ADS 6646 A 08 16 31.89 +79 30 07 ADS 6646 B 08 16 33.77 +79 30 27 ADS 8861 13 19.6 +35 07
Radial velocities and residuals ADS ADS name --- HJD Heliocentric Julian Date d RV Radial velocity km/s e_RV Formal error of radial velocity km/s O-C Residual to the orbit km/s Rem Remarks, see Note number=1 COR CORAVEL measurement Rejected in orbit computation --- appen.tex LaTeX version of appendix Patricia Bauer CDS 1996 May 23 Andrei Tokovinin, <toko@gag.observ-gr.fr> J_A+AS_121_71.xml Abundances for globular cluster giants. I. Homogeneous metallicities for 24 clusters J/A+AS/121/95 J/A+AS/121/95 Atmospheric parameters for 24 clusters Abundances for globular cluster giants. I. Homogeneous metallicities for 24 clusters E Carretta R G Gratton Astron. Astrophys. Suppl. Ser. 121 95 1997 1997A&AS..121...95C Abundances, [Fe/H] Effective temperatures globular clusters: general stars: abundances stars: Population II We have obtained high resolution, high signal-to-noise ratio CCD echelle spectra of 10 bright red giants in 3 globular clusters (47 Tuc, NGC 6752 and NGC 6397) roughly spanning the whole range of metallicities of the galactic globular cluster system. The analysis of this newly acquired material reveals no significant evidence of star-to-star variation of the [Fe/H] ratio in these three clusters. Moreover, a large set of high quality literature data (equivalent widths from high dispersion CCD spectra) was re-analyzed in an homogeneous and self-consistent way to integrate our observations and derive new metal abundances for more than 160 bright red giants in 24 globular clusters (i.e. about 16% of the known population of galactic globulars). This set was then used to define a new metallicity scale for globular clusters which is the result of high quality, direct spectroscopic data, of new and updated model atmospheres from the grid of Kurucz (1992), and of a careful fine abundance analysis; this last, in turn, is based on a common set of both atomic and atmospheric parameters for all the stars examined.
Atmospheric parameters and abundance analysis NGC NGC designation --- Name Star name --- Source Source for equivalent width --- Teff Effective Temperature (K) K logg Surface gravity cm/s2 [A/H] Abundance Sun Vel Microturbulent velocities km/s nFeI Number of FeI lines used --- logn(FeI) Absolute number density abundances of FeI --- e_logn(FeI) Sigma for Fe I abundances --- nFeII Number of FeII lines used --- logn(FeII) Absolute number density abundances of FeII --- e_logn(FeII) Sigma for Fe II abundances --- [Fe/H] Metallicity --- Patricia Bauer CDS 1996 Jun 03 Eugenio Carretta <CARRETTA@astbo3.bo.astro.it> J_A+AS_121_95.xml Stellar contents of the open clusters Be 64 and Be 69 J/A+AS/122/111 J/A+AS/122/111 Berkeley 64 and 69 stars UBVRI photometry Stellar contents of the open clusters Be 64 and Be 69 A K Pandey A K Durgapal B C Bhatt V Mohan H S Mahra Astron. Astrophys. Suppl. Ser. 122 111 1997 1997A&AS..122..111P Clusters, open Photometry, UBVRI Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Be 64, Be 69) We present UBVRI CCD photometry for previously unstudied open clusters (Be 64 and Be 69). Photometry has also been carried out for nearby fields to correct f or the effects of field stars contamination. From the colour-colour diagram the reddening for Be 64 and Be 69 is estimated to be ~1.05mag and ~0.65mag respectively. In case of Be 69 the comparison of observational colour-magnitude diagram (CMD) with the standard isochrones of VandenBerg (19855ApJS...58..711V) indicates an apparent discrepancy between the shape of the turnoff and isochrones. The morphological features of the CMDs of Be 69 are better understood in terms of convective overshooting. The comparison of CMDs of both the clusters with the convective overshoot models (Bertelli et al. 1994A&AS..106..275B) produces a good fit for a metallicity Z=0.008 and age =0.8-1.0Gyr. An apparent distance modulus (m-M)=16.2 and 14.3 has been estimated for Be 64 and Be 69, respectively, which corresponds to a distance of 3880+/-480pc and 2860+/-310pc, respectively.
Berkeley 64 C 0217+656 02 21.1 +65 54 Berkeley 69 C 0521+326 05 24.6 +32 39
Magnitudes and colours of the stars in the field of Be 64 Magnitudes and colours of the stars in the field of Be 69 (North + South regions) No Serial Number (starts by N or S for table3) --- Xpos X-coordinate pix Ypos Y-Coordinate pix Vmag V magnitude mag U-B U-B color index mag n_U-B No measure number=1 * indicates that the magnitude in the colour could not be obtained --- B-V B-V color index mag n_B-V No measure number=1 * indicates that the magnitude in the colour could not be obtained --- V-I V-I color index mag n_V-I No measure number=1 * indicates that the magnitude in the colour could not be obtained --- V-R V-R color index mag n_V-R No measure number=1 * indicates that the magnitude in the colour could not be obtained --- b64.ps Fig. 1. Identification map for the cluster Be 64 b69.ps Fig. 2. Identification map for the cluster Be 69 Patricia Bauer CDS 1996 Jul 25 A.K. Pandey <pandey@upso.ernet.in> J_A+AS_122_111.xml Spectroscopic survey of delta Scutit stars. I. Rotation velocities and effective temperatures. J/A+AS/122/131 J/A+AS/122/131 Delta Scuti rotational velocities and Teff Spectroscopic survey of delta Scutit stars. I. Rotation velocities and effective temperatures. E Solano J Fernley Astron. Astrophys. Suppl. Ser. 122 131 1997 1997A&AS..122..131S Effective temperatures Rotational velocities Stars, variable delta Scuti stars: fundamental parameters stars: rotation Projected rotational velocities and effective temperatures for 68 delta Sct stars as well as 41 non-variable stars of similar spectral type and luminosity are presented here. The observations were performed between 1990 and 1994 at two different observatories: the Observatorio del Roque de los Muchachos (La Palma, Spain) and the McDonald Observatory (Texas, USA).
Delta Scuti stars projected rotational velocities *Non-variable stars sample projected rotational velocities HD HD star number --- HR HR star number --- GCVS GCVS star designation (in table3 only) --- vsini Projected rotational velocity number=1 Value obtained using the method described in Gray (1992). For La Palma spectra, the line chosen for the v sin i calculation appears in the last column (Lambda). For McDonald spectra, the mean rotational velocity and the standard deviation are given in the forth column and the number of lines used is shown in the last column (Line). The absence of suitable lines prevents the calculation of for VW Ari and CY Aqr km/s e_vsini rms uncertainty on vsini km/s Lambda Spectral line 0.1nm u_Lambda Uncertainty flag on Lambda --- Delta Sct stars effective temperatures Non-variable stars sample effective temperatures HD HD star number --- HR HR star number --- GCVS GCVS star designation (only in table6) --- Note See note number=1 A '*' indicates stars that show variations in amplitude {DELTA}V>=0.06 which correspond to variations of {DELTA}T_eff_=100K --- TeffPJ Petersen & Jorgensen (1972A&A....17..367P) calibration number=2 Only in table6 K TeffPR Philip & Relyea (1979AJ.....84.1743P) calibration K TeffMD Moon & Dworetsky (1985) calibration K TeffLGKu Lester et al. (1986ApJS...61..509L) calibration (upper limit) K --- dash --- TeffLGKl Lester et al. (1986ApJS...61..509L) calibration (lower limit) K TeffB Balona (1994MNRAS.268..119B) calibration K TeffHbu Hbeta calibration (upper limit) K --- dash --- TeffHbl Hbeta calibration (2) (lower limit) K TeffHau Halpha calibration (2) (upper limit) K --- dash --- TeffHal Halpha calibration (2) (lower limit) K tables.tex LaTeX version of Tables 3, 4, 6, and 7. Patricia Bauer CDS 1996 Jul 30 Enrique Solano <ESM@v3600.vilspa.esa.es.> J_A+AS_122_131.xml Stark broadening of Ba I and Ba II spectral lines J/A+AS/122/163 J/A+AS/122/163 Ba I & Ba II Stark broadening Stark broadening of Ba I and Ba II spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 122 163 1997 1997A&AS..122..163D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles Using a semiclassical approach, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for 14 Ba I and 64 Ba II multiplets for perturber densities 10^15^-10^18^cm^-3^ and temperatures T=2500-50000K for BaI and 5000-100000K for Ba II. The results have been compared with available experimental and theoretical data.
Stark broadening parameters due to e-, p- and He II-impacts for Ba I Stark broadening parameters due to e-, p- and He II-impacts for Ba II N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe+ (4) --- WHe+ FWHM for He II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe+ (4) --- dHe+ shift for He II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1996 Jun 28 Milan S. Dimitrijevic <mdimitrijevic@aob.bg.ac.yu> J_A+AS_122_163.xml CCD photometry of variable stars in the field of the globular cluster NGC 6397 J/A+AS/122/1 J/A+AS/122/1 BV photometry of variables in NGC 6397 CCD photometry of variable stars in the field of the globular cluster NGC 6397 J Kaluzny Astron. Astrophys. Suppl. Ser. 122 1 1997 1997A&AS..122....1K Clusters, globular Photometry, UBV binaries: close blue stragglers globular clusters: individual (NGC 6397) Hertzsprung-Russell (HR diagram) stars: variables: other Tables 5 and 6 contain BV photometry of stars from NGC 6397 field which is presented in Figs. 1 and 2, respectively. File template.fits is a FITS format image of the surveyed field. Stars coordinates listed in the paper correspond to positions on this image.
NGC 6397 C 1736-536 17 40.9 -53 41
BV photometry of stars from the field of NGC 6397 presented in fig. 1 BV photometry of stars from the field of NGC 6397 presented in fig. 2 ID ID number --- Xpos X coordinate number=1 1 pixel=0.396 arcsec; X axis points toward West; Y axis points toward South pix Ypos Y coordinate number=1 1 pixel=0.396 arcsec; X axis points toward West; Y axis points toward South pix Vmag Vmagnitude mag e_Vmag rms uncertainty on Vmag mag o_Vmag number of averaged V measurements --- q_Vmag quality flag for V number=2 q=1 means relatively poor quality --- B-V B-V color index mag e_B-V rms uncertainty on B-V mag o_B-V number of averaged B measurements --- q_B-V quality flag for B-V number=2 q=1 means relatively poor quality --- *Phased V-band light curve Star Star name --- Phase Phase --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag HJD Heliocentric Julian date d *V-band light curve Star Star name --- HJD Heliocentric Julian date d Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag template.fit *FITS format image of the surveyed field The image size is 2048x2046 (8.39Mb) and it is written in a 16 bits/pixel format. Patricia Bauer CDS 1996 Jun 28 Janusz Kaluzny <jka@vela.astrouw.edu.pl> J_A+AS_122_1.xml The ROSAT Galactic Plane Survey: analysis of a low latitude sample area in Cygnus. The observations J/A+AS/122/201 J/A+AS/122/201 ROSAT Galactic Plane Survey observations The ROSAT Galactic Plane Survey: analysis of a low latitude sample area in Cygnus. The observations C Motch P Guillout F Haberl M W Pakull W Pietsch K Reinsch Astron. Astrophys. Suppl. Ser. 122 201 1997 1997A&AS..122..201M J/A+A/318/111 : The ROSAT Galactic Plane Survey (Motch+ 1997) Platais I., 1994BICDS..44....9P = Cat. <I/203> Radio sources stars: activity stars: neutron stars: statistics X-rays: general X-rays: stars The analysis of the part of the ROSAT all-sky survey covering the galactic plane is the scope of a dedicated project called the ROSAT Galactic Plane Survey. In order to statistically understand the nature of the =~14000 sources discovered by ROSAT at |b|<=20{deg}, a number of sample areas have been chosen for follow-up optical identification. In this paper we present the X-ray and optical material gathered in a region located in the Cygnus constellation, centered at l=90{deg}, b=0{deg} and covering an area of 64.5deg^2^. A total of 95 and 128 sources are detected with a maximum likelihood larger than 10 and 8 respectively. With a typical survey exposure time of the order of 700 to 900 s the flux completeness level is =~0.02cts/s corresponding to =~2x10^-13^erg/cm^2^/s. The position of the sample area allows to investigate the soft X-ray content of a rather typical region of the galactic plane. In this paper we describe the details of the observational procedures and data reduction. For each ROSAT source we list the main X-ray characteristics together with those of the proposed optical identification. When appropriate, we also show optical spectra and finding charts. The full analysis and discussion of these data are presented in a companion paper (Motch et al. 1997, Cat. <J/A+A/318/111>).
ROSAT
X-ray characteristics of ROSAT survey sources detected with ML>=8 in the Cygnus test region X-ray characteristics of ROSAT survey sources detected with 7<=ML<8 in the Cygnus test region Source Source index --- ROSAT ROSAT name --- RAh X-ray right ascension (J2000) h RAm X-ray right ascension (J2000) min RAs X-ray right ascension (J2000) s DEd X-ray declination (J2000) deg DEm X-ray declination (J2000) arcmin DEs X-ray declination (J2000) arcsec r90 90% confidence radius arcsec Count Count rate ct/s e_Count rms uncertainty on Count ct/s MaxLik Maximum likehood --- HR1 Hardness ratio 1 --- e_HR1 rms uncertainty on HR1 --- HR2 Hardness ratio 2 --- e_HR2 rms uncertainty on HR2 --- Optical properties of all proposed optical counterparts in the Cygnus test region for sources with ML>= 8 Optical properties of all proposed optical counterparts in the Cygnus test region for sources with 7<=ML< 8. Source Source index --- ROSAT ROSAT name --- Class Class of the proposed optical counterpart --- u_Class ? for the more uncertain cases number=1 Proposed counterparts having a probability of identification in the range 95% - 98%, These more uncertain cases are marked by a '?' in the u_IdOpt column and in the u_Class column --- IdOpt Optical identification number=1 Proposed counterparts having a probability of identification in the range 95% - 98%, These more uncertain cases are marked by a '?' in the u_IdOpt column and in the u_Class column --- u_IdOpt ? for the more uncertain cases number=1 Proposed counterparts having a probability of identification in the range 95% - 98%, These more uncertain cases are marked by a '?' in the u_IdOpt column and in the u_Class column --- SpType Spectral type --- Vmag V magnitude mag B-V B-V colour index mag RAh Optical right ascension (J2000) h RAm Optical right ascension (J2000) min RAs Optical right ascension (J2000) s n_RA n: Right ascension not available --- DEd Optical declination (J2000) deg DEm Optical declination (J2000) arcmin DEs Optical declination (J2000) arcsec n_DE n: Declination not available --- Dist Distance between X-ray and optical position in units of 90% confidence radius --- Notes on individual sources Source Source index --- ROSAT ROSAT name --- Com Comments --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Aug 12 Christian Motch <motch@cdsxb7.u-strasbg.fr> J_A+AS_122_201.xml Stroemgren uvby photometry of the magnetic chemically peculiar stars HD 32633, 25 Sex, HR 7224, and HD 200311 J/A+AS/122/249 J/A+AS/122/249 uvby photometry of 4 CP stars Stroemgren uvby photometry of the magnetic chemically peculiar stars HD 32633, 25 Sex, HR 7224, and HD 200311 S J Adelman Astron. Astrophys. Suppl. Ser. 122 249 1997 1997A&AS..122..249A J/A+AS/103/1 : 63 And, HD 192913, HR 8240 & 108 Aqr (Adelman+ 1994) J/A+AS/106/333 : Alpha And, HD 184905, HR 8216 & HR 8434 (Adelman+ 1994) J/A+AS/114/253 : HD11187, HD14940, HD15144, 20 Eri & HR8933 (Adelman+, 1995) J/A+AS/122/249 : HD 32633, 25 Sex, HR 7224 & HD 200311 (Adelman, 1997) J/A+AS/123/445 : uvby photometry of metallic & Hg-Mn stars (Adelman 1997) J/A+AS/125/65 : HD 37776, HR 2258, HR 6958 & 108 Aqr (Adelman 1997) J/PASP/109/9 : HR 1643, Theta Aur, 49 Cam, and HR 3724 (Adelman 1997) J/A+AS/125/497 : Theta Vir and 109 Vir uvby photometry (Adelman 1997) Photometry, uvby Stars, peculiar stars: chemically peculiar stars: individual (HD 32633, 25 Sex, HR 7224, HD 200311) Differential Stroemgren uvby photometric observations from the Four College Automated Photoelectric Telescope refine the rotational periods and define the shapes of the light curves of four magnetic Chemically Peculiar stars. HD 32633 (P=6.43000d) exhibits an in-phase variability with asymmetrically shaped light curves. 25 Sex (P=4.37900d) has a complex variability with the v, b, and y light variability crudely in phase, but quite different from that of u. HR 7224 (P=1.123095d) shows in-phase variability with two nearly equal secondary minima. HD 200311 (P=26.0042d), which was previous thought to be a long period variable, is found to be a modest photometric variable.
HD 32633 05 06 08.2 +33 55 09 HD 90044 25 Sex 10 23 26.6 -04 04 27 HR 7224 HD 177410 18 58 52.6 +69 31 50 HD 200311 21 01 14.1 +43 43 19
HD 32633 photometry 25 Sex photometry HR 7224 photometry HD 200311 photometry HJD Heliocentric Julian Date d umag1 Variable-comparison (v-c) u magnitude mag umag2 Check-comparison (ch-c) u magnitude mag vmag1 Variable-comparison (v-c) v magnitude mag vmag2 Check-comparison (ch-c) v magnitude mag bmag1 Variable-comparison (v-c) b magnitude mag bmag2 Check-comparison (ch-c) b magnitude mag ymag1 Variable-comparison (v-c) y magnitude mag ymag2 Check-comparison (ch-c) y magnitude mag Average photometry Name Star name --- Per Period considered number=1 For HD 32633 : year2: From 2448543.9111 to 2448546.9967 year3: From 2448546.9967 to 2449416.6549 year4: From 2449645.9468 to 2449792.6202 year5: From 2449986.8909 to 2450039.9390 For 25 Sex : year2: From 2448695.7385 to 2448721.7129 year4: From 2449009.7950 to 2449118.6704 year5: From 2449334.9544 to 2449470.6687 year6: From 2449684.9934 to 2449839.6589 For HR 7224 : year4: From 2449439.9787 to 2449548.7687 year5: From 2449611.6324 to 2449906.7026 For HD 200311: year3: From 2448805.9445 to 2449164.8044 year4: From 2449253.7114 to 2449547.7836 year5: From 2449611.6534 to 2449908.7685 --- umag1 Variable-comparison (v-c) u magnitude mag e_umag1 rms uncertainty on umag1 mag umag2 Check-comparison (ch-c) u magnitude mag e_umag2 rms uncertainty on umag2 mag vmag1 Variable-comparison (v-c) v magnitude mag e_vmag1 rms uncertainty on vmag1 mag vmag2 Check-comparison (ch-c) v magnitude mag e_vmag2 rms uncertainty on vmag2 mag bmag1 Variable-comparison (v-c) b magnitude mag e_bmag1 rms uncertainty on bmag1 mag bmag2 Check-comparison (ch-c) b magnitude mag e_bmag2 rms uncertainty on bmag2 mag ymag1 Variable-comparison (v-c) y magnitude mag e_ymag1 rms uncertainty on ymag1 mag ymag2 Check-comparison (ch-c) y magnitude mag e_ymag2 rms uncertainty on ymag2 mag Patricia Bauer CDS 1996 Jul 25 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> UNKNOWN UNKNOWN There were an inversion between the b and v magnitude labels. This was corrected on 24-Apr-1998 J_A+AS_122_249.xml Millimetre continuum measurements of extragalactic radio sources. IV: Data from 1993-1994. J/A+AS/122/271 J/A+AS/122/271 mm-monitoring of radio sources IV. Millimetre continuum measurements of extragalactic radio sources. IV: Data from 1993-1994. H -P Reuter C Kramer A Sievers G Paubert R Moreno A Greve S Leon J F Panis M Ruiz-Moreno H Ungerechts W Wild Astron. Astrophys. Suppl. Ser. 122 271 1997 1997A&AS..122..271R J/A+AS/102/611 : mm continuum of extragal. sources III. (Steppe+ 1993) Steppe H. et al., Paper I., 1988, A&AS 75, 317 =1988A&AS...75..317S Steppe H. et al., Paper II., 1992, A&AS 96, 441 =1992A&AS...96..441S Steppe H. et al., Paper III., 1993, A&AS 102, 611S =Cat. <J/A+AS/102/611> QSOs Radio sources BL Lacertae objects: general galaxies: active quasars: general radio continuum: general surveys Radio flux densities are presented for 118 extragalactic radio sources monitored at 90, 142 and 230GHz with the IRAM 30m telescope during 1993-1994. For the most frequently observed sources we show light curves including 30 m-measurements published in previous papers, Steppe et al. (1988A&AS...75..317S; 1992A&AS...96..441S and and 1993, Cat. <J/A+AS/102/611>)
Pointing sources used at the IRAM 30m telescope Source Source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Strength Source strength indicator at 90 GHz number=1 Source strength: s = strong (> 3.0 Jy) m = medium (1 - 3 Jy) w = weak (< 1 Jy) --- Note An 'X' indicates that the light curve for the source is shown in Fig. 1 --- List of flux densities at 1, 2 and 3 mm QSO QSO name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec OBSdate Observing date yr Freq Observing frequency GHz S Flux density Jy e_S rms uncertainty on flux density Jy Patricia Bauer CDS 1996 Oct 07 Hans-Peter Reuter <reuter@mpifr-bonn.mpg.de> J_A+AS_122_271.xml Extendend VCS Stark broadening tables for hydrogen-Lyman to Brackett series J/A+AS/122/285 J/A+AS/122/285 VCS Stark broadening tables for hydrogen Extendend VCS Stark broadening tables for hydrogen-Lyman to Brackett series M Lemke Astron. Astrophys. Suppl. Ser. 122 285 1997 1997A&AS..122..285L VI/82 : Stark broadening of H lines (Stehle 1995) Atomic physics atomic data line: profiles Stark profiles computed with the VCS theory are presented here for the Lyman, Balmer, Paschen, and Brackett series of hydrogen. They cover the series up to n=22 and a wide range of temperature and electron density. Both Doppler broadened profiles (as applicable to stellar atmospheres) and unbroadened profiles are given.
log Delta Alpha Min for all lines in the Doppler broadened tables (all series) Serie Name of the serie number=1 Ly: Lyman, Ba: Balmer, Pa: Paschen, Br: Brackett --- lq Lower quantum number --- uq Upper quantum number --- log(DalphaMin) Detuning from minimum central wavelength --- Patricia Bauer CDS 1996 Aug 05 Michael Lemke <ai26@a400.sternwarte.uni-erlangen.de> J_A+AS_122_285.xml K and evolutionary corrections from UV to IR J/A+AS/122/399 J/A+AS/122/399 K and evolutionary corrections K and evolutionary corrections from UV to IR B M Poggianti Astron. Astrophys. Suppl. Ser. 122 399 1997 1997A&AS..122..399P Galaxies, photometry Models, evolutionary cosmology: miscellaneous galaxies: distances and redshifts galaxies: evolution galaxies: fundamental parameters galaxies: photometry K and evolutionary corrections are given for the E, Sa and Sc Hubble types for the U, B, V, R, I, J, H, K filters of the Johnson-Bessell & Brett photometric system and the gri filters of the modified Thuan & Gunn system up to the redshift z=3. Their dependence on the time scale of star formation in ellipticals is investigated. The corrections are computed according to an evolutionary synthesis model that reproduces the integrated galaxy spectrum in the range 1000-25000{AA}; such a model makes use of an infrared observed stellar library and its results are compared with nearby galaxies. Evolving spectral energy distributions of the various Hubble types, as well as optical-IR and IR-IR colour evolution and adopted filter response functions are also given.
*Logarithm of the flux for different SED models Lam Wavelength 0.1nm logF(Lam)3 Flux for model SED of a 15 Gyr old elliptical --- logF(Lam)4 Flux for model SED of a 15 Gyr old Sa --- logF(Lam)5 Flux for model SED of a 15 Gyr old Sc --- logF(Lam)6 Flux for model SED: E of age 13.2 Gyr (z=0.1) --- logF(Lam)7 Flux for model SED: E of age 10.6 Gyr (z=0.3) --- logF(Lam)8 Flux for model SED: E of age 8.7 Gyr (z=0.5) --- logF(Lam)9 Flux for model SED: E of age 7.4 Gyr (z=0.7) --- logF(Lam)10 Flux for model SED: E of age 5.9 Gyr (z=1.0) --- logF(Lam)11 Flux for model SED: E of age 4.3 Gyr (z=1.5) --- logF(Lam)12 Flux for model SED: E of age 3.4 Gyr (z=2.0) --- logF(Lam)13 Flux for model SED: E of age 2.2 Gyr (z=3.0) --- logF(Lam)14 Flux for model SED: Sa of age 13.2 Gyr --- logF(Lam)15 Flux for model SED: Sa of age 10.6 Gyr --- logF(Lam)16 Flux for model SED: Sa of age 8.7 Gyr --- logF(Lam)17 Flux for model SED: Sa of age 7.4 Gyr --- logF(Lam)18 Flux for model SED: Sa of age 5.9 Gyr --- logF(Lam)19 Flux for model SED: Sa of age 4.3 Gyr --- logF(Lam)20 Flux for model SED: Sa of age 3.4 Gyr --- logF(Lam)21 Flux for model SED: Sa of age 2.2 Gyr --- logF(Lam)22 Flux for model SED: Sc of age 13.2 Gyr --- logF(Lam)23 Flux for model SED: Sc of age 10.6 Gyr --- logF(Lam)24 Flux for model SED: Sc of age 8.7 Gyr --- logF(Lam)25 Flux for model SED: Sc of age 7.4 Gyr --- logF(Lam)26 Flux for model SED: Sc of age 5.9 Gyr --- logF(Lam)27 Flux for model SED: Sc of age 4.3 Gyr --- logF(Lam)28 Flux for model SED: Sc of age 3.4 Gyr --- logF(Lam)29 Flux for model SED: Sc of age 2.2 Gyr --- K corrections in the V band from this paper and from Pence (1976ApJ...203...39P) z Redshift --- E K correction for E (1Gyr) model mag E/S0 K correction for E/S0 Pence observations mag Sa K correction for Sa model mag Sab K correction for Sab Pence observations mag Sc K correction for Sc model mag Sbc K correction for Sbc Pence observations mag *K corrections *Evolutionary corrections z Redshift --- Filt Filter --- E Correction in band Filt for E (1Gyr) model mag E2 Correction in band Filt for E2 (1.4Gyr) model mag Sa Correction in band Filt for Sa model mag Sc Correction in band Filt for Sc model mag Filter response functions Filt Filter --- Lambda Wavelength 0.1nm Resp Response --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Aug 06 Bianca Poggianti <bianca@magellan.astro.rug.nl> J_A+AS_122_399.xml A photometric catalogue of the Coma cluster core J/A+AS/122/409 J/A+AS/122/409 Photometric catalogue of Coma A photometric catalogue of the Coma cluster core C Lobo A Biviano F Durret D Gerbal O Le Fevre A Mazure E Slezak Astron. Astrophys. Suppl. Ser. 122 409 1997 1997A&AS..122..409L Clusters, galaxy Photometry, CCD galaxies: clusters: individual (Coma cluster) galaxies: luminosity function, mass function galaxies: photometry We present a CCD catalogue of 7023 galaxies and 4096 stars in the region of the Coma cluster containing positions, central surface brightnesses and V magnitudes (isophote 26.5). We estimate that data is complete up to isophotal V magnitude 22.5 and the surface brightness limiting detection value is approximately 24 mag/arcsec2.
Photometric catalogue of Coma RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec r26.5 Isophotal radius arcsec mu0 Central surface brightness mag/arcsec2 V26.5 Isophotal apparent V magnitude mag |deltaV| Magnitude error (in modulus) mag Type Classification number=1 Classification of the object as follows: 1: Star 0: Galaxy --- nGMP GMP number <VII/42> number=2 GMP number, when available. The correspondence was obtained by cross-correlating positions, which results in inevitable ambiguities in some cases. That is why there are 4 entries doubled. In addition, there are also several other entries which are attributed the same GMP number. Details are given in the paper. --- Cat GMP catalogue number=3 GMP catalogue used for the matching: g: Godwin J.G., Metcalfe N., Peach J.V., <VII/42> GMP galaxy catalog s: GMP unpublished star catalog --- Xarcsec GMP abscissa corrected to GSC arcsec Yarcsec GMP ordinate corrected to GSC arcsec HRV Heliocentric radial velocity number=4 Heliocentric radial velocity are taken from: Biviano A., Durret F., Gerbal D. et al., <J/A+AS/111/265> km/s Patricia Bauer CDS 1996 Aug 27 Catarina Lobo <lobo@iap.fr> J_A+AS_122_409.xml Monitoring MWC 560 = V694 Mon in 1990-1995. II. Plate spectra J/A+AS/122/43 J/A+AS/122/43 V694 Mon plate spectra Monitoring MWC 560 = V694 Mon in 1990-1995. II. Plate spectra T Tomov D Kolev Astron. Astrophys. Suppl. Ser. 122 43 1997 1997A&AS..122...43T J/A+AS/116/1 : UBV photometry of MWC560 Equivalent widths Radial velocities Stars, variable accretion, accretion disks binaries: symbiotic stars: activity stars: individual (MWC 560) stars: mass-loss We present the results of the photographic spectral observations of MWC560 carried out in the period 1990-1993. The evolution of the spectrum, the changes in the radial velocities of the different line systems, as well as the variations in the equivalent widths of the different Balmer absorption components, are given and briefly discussed. The suggestion that the hot component of MWC560 ejects high-velocity, highly-collimated jets along the line of sight, is in very good agreement with the observations. All the results, including the variations in the shapes, velocities and equivalent widths of the strong-shifted Balmer absorptions, confirm that compact companion in MWC560 ejects matter in two different regimes - discrete and quasi-stationary. It is supposed that the permanent presence of a relatively weak and small-shifted Balmer absorption component in the spectrum, indicates additional persistent, not spherically symmetric matter outflow.
MWC 560 V694 Mon 07 23 25.9 -07 38 03
*Slowest Balmer absorption components data OBSdate Date of the observation "DD/MM/YY" JD Julian date of the observation d RVHb Hbeta radial velocity km/s u_RVHb Uncertainity flag on RVHb --- WHb Hbeta equivalent width 0.1nm u_WHb Uncertainity flag on WHb --- RVHg Hgamma radial velocity km/s l_WHg Limit flag on WHg --- WHg Hgamma equivalent width 0.1nm u_WHg Uncertainity flag on WHg --- RVHd Hdelta radial velocity km/s WHd Hdelta equivalent width 0.1nm u_WHd Uncertainity flag on WHd --- RVHe Heps radial velocity km/s u_RVHe Uncertainity flag on RVHe --- WHe Heps equivalent width 0.1nm u_WHe Uncertainity flag on WHe --- RVH8 H8 radial velocity km/s u_RVH8 Uncertainity flag on RVH8 --- WH8 H8 equivalent width 0.1nm u_WH8 Uncertainity flag on WH8 --- RVH9 H9 radial velocity km/s u_RVH9 Uncertainity flag on RVH9 --- WH9 H9 equivalent width 0.1nm u_WH9 Uncertainity flag on WH9 --- RVH10 H10 radial velocity km/s WH10 H10 equivalent width 0.1nm u_WH10 Uncertainity flag on WH10 --- RVH11 H11 radial velocity km/s WH11 H11 equivalent width 0.1nm u_WH11 Uncertainity flag on WH11 --- RVH12 H12 radial velocity km/s WH12 H12 equivalent width 0.1nm RVH13 H13 radial velocity km/s WH13 H13 equivalent width 0.1nm RVH14 H14 radial velocity km/s WH14 H14 equivalent width 0.1nm *Different line systems heliocentric radial velocities OBSdate Date of the observation "DD/MM/YY" JD Julian date of the observation d RV1 Radial velocity of the SSBA components number=1 SSBA = Strong-shifted Balmer absorptions km/s u_RV1 Uncertainity flag on RV1 --- e_RV1 rms uncertainty on RV1 km/s o_RV1 Number of the measured lines --- RV2 Balmer emission components radial velocity km/s e_RV2 rms uncertainty on RV2 km/s o_RV2 Number of the measured lines --- RV3 CaII K strong-shifted abs. radial velocity km/s u_RV3 Uncertainity flag on RV3 --- n_RV3 Note number=2 a: The strong-shifted absorption component of CaII K line is blended with one of the absorption components of the Balmer line H8. --- RV4 Ionized metals absorptions radial velocity km/s u_RV4 Uncertainity flag on RV4 --- RV5 Ionized metals emissions radial velocity km/s e_RV5 rms uncertainty on RV5 km/s o_RV5 Number of the measured lines --- Strong-shifted Balmer absorption components EW OBSdate Date of the observation "DD/MM/YY" JD Julian date of the observation d WHb Hbeta equivalent width 0.1nm WHg Hgamma equivalent width 0.1nm WHd Hdelta equivalent width 0.1nm WHe Heps equivalent width 0.1nm WH8 H8 equivalent width 0.1nm u_WH8 Uncertainity flag on WH8 --- WH9 H9 equivalent width 0.1nm WH10 H10 equivalent width 0.1nm u_WH10 Uncertainity flag on WH10 --- WH11 H11 equivalent width 0.1nm u_WH11 Uncertainity flag on WH11 --- WH12 H12 equivalent width 0.1nm WH13 H13 equivalent width 0.1nm u_WH13 Uncertainity flag on WH13 --- WH14 H14 equivalent width 0.1nm WH15 H15 equivalent width 0.1nm Patricia Bauer CDS 1996 Jul 30 T. Tomov <rozhen@tempus.tu-plovdiv.bg> J_A+AS_122_43.xml New proper-motion stars with declination between -5deg and-30deg and right ascension between 9h and 13h30m J/A+AS/122/447 J/A+AS/122/447 New proper-motion stars -30<DE<-5, 9<RA<13h30m New proper-motion stars with declination between -5deg and-30deg and right ascension between 9h and 13h30m H Wroblewski C Torres Astron. Astrophys. Suppl. Ser. 122 447 1997 1997A&AS..122..447W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/78/231 : Dec<-40, 0<RA<4h30, stars 1 to 144 (Wroblewski+ 1989) J/A+AS/91/129 : Dec<-40, 0<RA<4h30, stars 145 to 521 (Wroblewski+ 1991) J/A+AS/105/179 : Dec<-40, 16<RA<24h, stars 522 to 1069 (Wroblewski+ 1994) J/A+AS/115/481 : -30<DE<-5, 0<RA<9h, stars 1070 to 1563 (Wroblewski+ 1996) J/A+AS/83/317 : LTT stars, Dec<-40, 0<RA<4h30 (Wroblewski+ 1990) J/A+AS/92/449 : LTT stars, Dec<-40, 4h30<RA<16h (Wroblewski+ 1992) J/A+AS/110/27 : LTT stars, Dec<-40, 16<RA<24h (Wroblewski+, 1995) Luyten W.J. 1957, A Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motions Exceeding 0.2 arcsec Annualy (The Lund Press, Minneapolis, Minnesota). Luyten W.J. 1979, LHS Catalogue, University of Minnesota, Minneapolis, Minnesota. (Cat. <I/87>) Proper motions astrometry Galaxy: halo stars: kinematics Data are given for 492 new stars with proper motion larger than 0.15arcsec/year found on 21 areas covering 25 square degrees each. These are located between -5deg and -30deg in declination and between 9h and 13h30m in right ascension. Photographic magnitudes range from 9.5 to 18.5. Four stars have proper motions larger than 0.5arcsec/year, in a magnitude range between 15.5 and 17.5.
Positions and relative proper motions WT Running number --- Loc Localisation (area and number) --- mpg Photographic magnitude, accurate to 0.5mag mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RAh2000 Right Ascension 2000 (hours) h RAm2000 Right Ascension 2000 (minutes) min RAs2000 Right Ascension 2000 (seconds) s DE-2000 Declination 2000 (sign) --- DEd2000 Declination 2000 (degrees) deg DEm2000 Declination 2000 (minutes) arcmin DEs2000 Declination 2000 (seconds) arcsec pm Total proper motion arcsec/yr e_pm Mean error on pm arcsec/yr pmPA Position angle (North to East) of the proper motion in J2000 equinox deg Remark Remarks number=1 4 : when proper-motion is the mean of #4 pairs of plates, k: probably companion of LTT 3462 l: probably companion of LTT 3528 m: probably companion of Perth 10627 --- James Marcout, Patricia Bauer CDS 1997 Jun 24 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_122_447.xml Carbon stars in the halo of the Magellanic Clouds: Identification and radial velocity data. J/A+AS/122/463 J/A+AS/122/463 Carbon stars in Magellanic Clouds Carbon stars in the halo of the Magellanic Clouds: Identification and radial velocity data. W E Kunkel M J Irwin S Demers Astron. Astrophys. Suppl. Ser. 122 463 1997 1997A&AS..122..463K Magellanic Clouds Radial velocities Stars, carbon Magellanic Clouds stars: carbon techniques: radial velocities The 16 tables list the heliocentric and galactocentric radial velocities of several hundred carbon stars in the halo of the LMC and SMC. Most of them are newly discovered stars.
Magellanic Cloud periphery carbon stars Table Number of the table in the paper --- Name Name of star --- Id Identification from field --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg HRV Heliocentric radial velocity km/s gRV Galactocentric radial velocity km/s q_HRV Quality parameter --- Spect Number of spectra --- Rmag R magnitude mag B-R B-R colour index mag Com Comments --- Inter Cloud carbon stars Magellanic Cloud periphery carbon stars Table Number of the table on the paper --- Name Name of star --- n_Name Note on Name number=1 * Stars observed by Hardy et al. (1989ApJ...344..210H), I magnitude is given. --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec GLAT Galactic longitude deg GLON Galactic latitude deg HRV Heliocentric radial velocity km/s gRV Galactocentric radial velocity km/s q_HRV Quality parameter --- N Number of spectra --- Vmag V magnitude mag B-V B-V colour index mag Com Comments --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Jul 30 Serge Demers <demers@ASTRO.UMontreal.CA> J_A+AS_122_463.xml NTT V, I, z photometry of the metal-rich bulge globular cluster Terzan 6 J/A+AS/122/483 J/A+AS/122/483 Terzan 6 NTT VI photometry NTT V, I, z photometry of the metal-rich bulge globular cluster Terzan 6 B Barbuy S Ortolani E Bica Astron. Astrophys. Suppl. Ser. 122 483 1997 1997A&AS..122..483B Clusters, globular Photometry globular clusters: general globular clusters: individual (Terzan 6) Hertzsprung-Russell (HR diagram) We present for the first time optical (V, I and Gunn z) colour magnitude diagrams for Terzan 6, which were collected under excellent seeing conditions with the ESO NTT telescope. The horizontal branch morphology is red, nearly superimposed on the red giant branch. The red giant branch morphology presents characteristics intermediate between those of 47 Tuc and NGC 6528/NGC 6553. We derive a reddening of E(B-V)=2.24 and a distance d_{sun}_=7.0kpc (assuming R=3.1). We conclude that Terzan 6 belongs to the metal-rich bulge globular cluster system.
Terzan 6 C 1747-312 17 50.7 -31 17
V, I photometry of Terzan 6 Seq Sequence number --- Xpos X pixel coordinate as in Fig. 1 pix Ypos Y pixel coordinate as in Fig. 1 pix Rad Radius pix Vmag V magnitude mag V-I V-I color index mag Patricia Bauer CDS 1996 Sep 19 Beatriz Barbuy <BARBUY@mesioa.obspm.fr> J_A+AS_122_483.xml New infrared carbon stars in the IRAS Point Source Catalog J/A+AS/122/489 J/A+AS/122/489 New infrared carbon stars in IRAS PSC New infrared carbon stars in the IRAS Point Source Catalog F Guglielmo N Epchtein F Arditti F Sevre Astron. Astrophys. Suppl. Ser. 122 489 1997 1997A&AS..122..489G Photometry, infrared Stars, carbon circumstellar matter Galaxy: stellar content infrared: stars stars: AGB and post-AGB stars: carbon stars: late-type We present new results of a search for infrared carbon stars (IRCS) based on the combination of IRAS and near infrared colours. A sample of 207 stars with IRAS colours that characterize IRCS is selected and measured in the JHKL photometric bands. Using a [12-25] vs. K-L colour diagram, 20 new IRCS candidates are proposed. Medium resolution spectra in the ~6000-9000{AA} range of 8 of these candidates confirm their carbon rich nature. In addition we propose a few stars with LRS class "4n" as oxygen-rich candidates, and a few stars with LRS classes "0n" and "1n" as carbon-rich.
IRAS
New infrared photometric data IRAS IRAS <II/125> name --- n_IRAS * indicates possible contamination of the near IR fluxes by a nearby star --- OBS Code for the epoch of the observation number=1 1: epoch 27-01-92 to 04-02-92 2: epoch 02-08-92 to 17-08-92 3: epoch 19-11-92 to 01-12-92 4: epoch 14-02-93 to 26-02-93 --- Kmag K magnitude mag J-K J-K color index mag H-K H-K color index mag K-L K-L color index mag [12-25] IRAS [12-25] color index number=2 The IRAS colours are defined using the magnitude scale given in the IRAS Explanatory Supplement (IRAS Science Team, 1987) mag [25-60] IRAS [25-60] color index number=2 The IRAS colours are defined using the magnitude scale given in the IRAS Explanatory Supplement (IRAS Science Team, 1987) mag LRS IRAS Low-Resolution Spectral type --- Class Classification in our system, Epchtein et al., (1987A&AS...71...39E) --- VH Classification in van der Veen and Habing (1988) system --- Id Identification in other catalogues number=3 The flags indicate that the objects have an entry in one or several of the following catalogs: C: GCCCS General Catalog of Cool Carbon Stars <III/156> S: General Catalog of S Stars <III/168> G: GSC General Catalog of S Stars <VII/116> I: another stellar catalog quoted in the IRAS PSC M: detected in one or several radio lines CO/HCN (Loup et al., 1993A&AS...99..291L) H2O maser (Comoretto et al., 1990A&AS...84..179C) OH maser (te Lintel-Hekkert et al., 1989A&AS...78..399T) More detailed information is given in Table 3. --- List of reference catalogs used IRAS IRAS <II/125> name --- GCVS GCVS designation <II/139> --- TMSS TMSS designation <II/2> --- RAFGL RAFGL designation <II/94> --- m_RAFGL Multiplicity index on RAFGL name --- GCCCS GCCCS designation <III/156> --- n_GCCCS S indicates that GCCCS contains designation from General Catalog of S Stars <III/168> --- GSC1 GSC SMR No <VII/116> --- GSC2 No <VII/116> --- Others Other names number=1 DO: Dearborn Observatory Catalogue of Faint Red Stars <II/68> SAO: Smithsonian Astrophysical Observatory Star Catalog <I/131> NSV: New Catalogue of Suspected Variable Stars <II/140> --- table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 Patricia Bauer CDS 1996 Aug 29 Francois Guglielmo <guglielm@iap.fr> J_A+AS_122_489.xml Kinematics of carbon stars in the outer regions of the Small Magellanic Cloud J/A+AS/122/507 J/A+AS/122/507 Kinematics of SMC carbon stars Kinematics of carbon stars in the outer regions of the Small Magellanic Cloud D Hatzidimitriou B F Croke D H Morgan R D Cannon Astron. Astrophys. Suppl. Ser. 122 507 1997 1997A&AS..122..507H J/A+AS/97/603 : C stars in SMC (RAW93) J/A+AS/113/539 : A survey of carbon stars in the SMC (Morgan+, 1995) Magellanic Clouds Stars, carbon galaxies: kinematics and dynamics Magellanic Clouds stars: carbon We present a radial velocity survey of a sample of the field population of carbon stars in the outer parts of the Small Magellanic Cloud (SMC). This first set of results includes radial velocities for 71 carbon stars, with an individual precision of +/-2-5km/s. The mean heliocentric velocity of the stars (excluding one very high velocity star) is 149.3+/-3.0km/s with a velocity dispersion of 25.2+/-2.1km/s. These values drop to 145.5+/-2.7km/s and 20.6+/-1.9km/s respectively, if we exclude the stars belonging to the Outer Wing. The velocity distribution does not show the multiple peaks seen in some samples of Population I objects. The mass of the SMC as inferred from the above velocity dispersion (without the outer Wing stars) is =~1.2x10^9^M_{sun}_.
The sample of SMC carbon stars observed *The sample of 16 LMC stars MH Star name number=1 In table1a, names from the Morgan and Hatzidimitriou (1995, Cat. <J/A+AS/113/539>) catalogue --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Dist Projected radial distance of each star from the dynamical centre of the SMC number=2 1 degree corresponds to approximately 1kpc at the distance of the SMC deg o_Dist Number of observations secured in each case --- HRV Derived heliocentric radial velocity (LSR) km/s ccp Height of the cross-correlation peak --- Obs Run during which the observations were made --- table1.tex LaTex version of table1 Patricia Bauer CDS 1996 Sep 03 Despina Hatzidimitriou <dh@physics.uch.gr> J_A+AS_122_507.xml A calibration of Geneva photometry for B to G stars in terms of Teff, logg, and [M/H] J/A+AS/122/51 J/A+AS/122/51 B to G stars calibration in Geneva photometry A calibration of Geneva photometry for B to G stars in terms of Teff, logg, and [M/H] M Kunzli P North R L Kurucz B Nicolet Astron. Astrophys. Suppl. Ser. 122 51 1997 1997A&AS..122...51K Models, atmosphere Photometry, Geneva stars: atmospheres stars: fundamental parameters stars: general We have used recent Kurucz models and many standard stars to revise previous calibrations of the Geneva photometric parameters in terms of Teff, logg, and [M/H]. In addition, new parameters pT and pG were defined, which are the Geneva equivalents of Stromgren's a and r parameters and allow to estimate Teff and logg for stars with intermediate temperature (spectral type A0-A3). A fortran code (calib.f) has been written, which applies our calibration to stars measured in the Geneva system. A conspicuous change in slope appears in the grid d vs B2-V1. It seems to be linked with the onset of convection in the superficial layers of the star's envelope.
The Geneva colours (uncorrected) of the Kurucz models Teff Effective temperature K logg Surface gravity cm/s2 [M/H] Metallicity Sun [U-B] Geneva [U-B] index mag [V-B] Geneva [V-B] index mag [B1-B] Geneva [B1-B] index mag [B2-B] Geneva [B2-B] index mag [V1-B] Geneva [V1-B] index mag [G-B] Geneva [G-B] index mag calib.doc *Notes about the code calib bcdci, bcmci, ptpgm10i, ptpgp00i, ptpgp10i, xcycm10i, xcycp00i and xcycp10i files contain the numerical values of the corrected grids and are necessary to use the code calib. Patricia Bauer CDS 1996 Aug 19 Marc Kunzli <marc.kunzli@obs.unige.ch> J_A+AS_122_51.xml Kinematical data on early-type galaxies. I. J/A+AS/122/521 J/A+AS/122/521 Kinematical data on early-type galaxies. I. Kinematical data on early-type galaxies. I. F Simien P Prugniel Astron. Astrophys. Suppl. Ser. 122 521 1997 1997A&AS..122..521S J/A+AS/126/15 : Kinematical data on early-type galaxies. II. (Simien+ 1997) J/A+AS/126/519 : Kinematical data on early-type galaxies. III. (Simien+ 1997) Galaxies, rotation Radial velocities Velocity dispersion galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: kinematics and dynamics As part of an ongoing program on the main parameters of early-type galaxies, we have performed long-slit absorption spectroscopy on a sample of 21 ellipticals and S0s. We present determinations of the central velocity dispersion and, for 18 objects, velocity-dispersion profiles and rotation curves.
Catalog elements for program galaxies Name Object identification number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 --- MType Morphological type number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 --- RAh Right Ascension 1950 (hours) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 h RAm Right Ascension 1950 (minutes) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 min RAs Right Ascension 1950 (seconds) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 s DE- Declination 1950 (sign) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 --- DEd Declination 1950 (degrees) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 deg DEm Declination 1950 (minutes) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 arcmin DEs Declination 1950 (seconds) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 arcsec RV Heliocentric radial velocity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 km/s BT Integrated blue magnitude number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 mag Dist Distance modulus number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 mag Re Effective radius number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 arcsec Eps Ellipticity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 --- PA Position angle of slit PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 deg r_Eps Reference for Eps and PA 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 --- Sig0 Central velocity dispersion number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 km/s e_Sig0 Error on Sig0 number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 km/s l_Vmax Upper-limit flag on Vmax number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 --- Vmax Maximum rotational velocity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 km/s e_Vmax Error on Vmax number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) 5 = references 3 and 4 km/s Log of the observations Name Object identification --- Date Date of observation "DD/MM/YY" PA Position angle of slit number=1 PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). deg Nexp Number of exposures --- Texp Exposure time min Seeing Seeing FWHM arcsec u_Seeing Uncertainty flag on Seeing --- Kinematical results (central values) Name Object identification --- HRV Heliocentric radial velocity km/s e_HRV Mean error on HRV km/s sig0 Central velocity dispersion number=1 Rotation and dispersion velocities are projected along the line of sight km/s u_sig0 Uncertainty flag on sig0 --- e_sig0 Mean error on sig0 km/s l_Vmax Upper-limit flag on Vmax --- Vmax Maximum rotational velocity number=1 Rotation and dispersion velocities are projected along the line of sight km/s e_Vmax Mean error on Vmax km/s rmax Radius corresponding to Vmax arcsec Profiles of velocity dispersion and rotation Name Object identification --- PA Position angle of slit (North --> East) number=1 PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg r Radius (<0 and >0 on opposite semi-axes) number=1 PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. arcsec Vrot Projected mean stellar rotation velocity number=2 rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. km/s e_Vrot Mean error on Vrot km/s sigma Projected velocity dispersion number=2 rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. km/s e_sigma Mean error on sigma km/s Patricia Bauer CDS 1996 Oct 31 Francois Simien <simien@obs.univ-lyon1.fr> Observatoire de Lyon F-69561 SAINT-GENIS-LAVAL cedex, France UNKNOWN UNKNOWN The files table3 and table have been updated on 12 June 1997, with the following changes: - object names are written without blank character, - a convention on the PA angles has been introduced to coincide with that adopted in the subsequent papers of the series. The galaxies for which PA changes are: NGC 97, 1426, 1713, 2332, 2685, 2732, 2768, 3193, 3818, 4434, 4476, 4478, 7660, and 7727, and UGC 3696. - minor format modifications have been made, again to conform to the formats adopted in the subsequent papers. Since the new convention on PA has incidence on the printed version of Table 2, we are enclosing an additional file, table2, which presents the log of the observations with the new values, and which may be useful to the readers. J_A+AS_122_521.xml Radio stars for linking celestial reference frames J/A+AS/122/529 J/A+AS/122/529 Radio stars for linking celestial reference frames Radio stars for linking celestial reference frames H G Walter R Hering C de Vegt Astron. Astrophys. Suppl. Ser. 122 529 1997 1997A&AS..122..529W Radio sources astrometry catalogs radio continuum: stars reference frames Radio stars play a key role in establishing the link between optical reference frames and the conventional celestial reference frame based on extragalactic radio sources. The relevant astrometric, astrophysical and radio quantities are compiled of 66 cardinal radio stars currently suited to frame connection and main tenance of the link. The catalogue entries are supplied with ample bibliographical codes and annotations for easy data retrieval.
Names from Simbad database No Star number --- Name1 Name from Simbad database --- Name2 Other name from Simbad database --- Name3 Other name from Simbad database --- Name4 Other name from Simbad database number=1 For No 1022, Name GT 0236+610 is from Ref.0040 --- Name5 Other name from Simbad database --- Name6 Other name from Simbad database --- Name7 Other name from Simbad database --- Name8 Other name from Simbad database --- Name9 Other name from Simbad database --- Name10 Other name from Simbad database --- Name11 Other name from Simbad database --- Name12 Other name from Simbad database --- Name13 Other name from Simbad database --- Name14 Other name from Simbad database --- Name15 Other name from Simbad database --- Name16 Other name from Simbad database --- Name17 Other name from Simbad database --- Name18 Other name from Simbad database --- Name19 Other name from Simbad database --- Name20 Other name from Simbad database --- Name21 Other name from Simbad database --- Name22 Other name from Simbad database --- Name23 Other name from Simbad database --- Optical positions No Star number --- RAh Optical right ascension (J2000) h RAm Optical right ascension (J2000) min RAs Optical right ascension (J2000) s e_RAs rms uncertainty on RAs 10-6s DE- Declination sign --- DEd Optical declination (J2000) deg DEm Optical declination (J2000) arcmin DEs Optical declination (J2000) arcsec e_DEs rms uncertainty on DEs 10-5arcsec EpochRA Observation epoch in right ascension yr EpochDE Observation epoch in declination yr Ref Bibliographic reference to the reference system of positions (usually the FK5 system) --- r_Pos Bibliographic reference to position --- Radio positions No Star number --- RAh Radio right ascension (J2000) h RAm Radio right ascension (J2000) min RAs Radio right ascension (J2000) s e_RAs rms uncertainty on RAs 10-6s DE- Declination sign --- DEd Radio declination (J2000) deg DEm Radio declination (J2000) arcmin DEs Radio declination (J2000) arcsec e_DEs rms uncertainty on DEs 10-5arcsec Epoch Epoch of observation yr Ref Bibliographic reference to the reference system of positions --- r_Pos Bibliographic reference to position --- Optical and radio proper motions and parallaxes radial velocities No Star number --- pmRAO Optical proper motion in right ascension number=1 The equinox of reference system for optical data is 2000.0 10-6s/yr e_pmRAO rms uncertainty on pmRAO 10-5arcsec/yr pmDEO Optical proper motion in declination number=1 The equinox of reference system for optical data is 2000.0 10-5arcsec/yr e_pmDEO rms uncertainty on pmDEO 10-5arcsec/yr r_pmO Bibliographic reference to proper motion number=2 The reference to the reference system of optical proper motions is FK5 --- pmRAR Radio proper motion in right ascension 10-6s/yr e_pmRAR rms uncertainty on pmRAR 10-5arcsec/yr pmDER Radio proper motion in declination number=1 The equinox of reference system for optical data is 2000.0 10-5arcsec/yr e_pmDER rms uncertainty on pmDER 10-5arcsec/yr RefR Bibliographic reference to the reference system of radio proper motions --- r_pmR Bibliographic reference to radio proper motion --- plxO Optical parallax 10-5arcsec e_plxO rms uncertainty on plxO 10-5arcsec r_plxO Reference for plxO --- plxR Radio parallax 10-5arcsec e_plxR rms uncertainty on plxR 10-5arcsec r_plxR Reference for plxR --- RV Radial velocity km/s e_RV rms uncertainty on RV km/s r_RV Radial velocity reference --- Photometry No Star number --- Vmag Apparent V magnitude for non-variable stars mag r_Vmag Vmag reference --- magMax Maximun apparent magnitude mag magMin Minimun apparent magnitude mag Band Band of the apparent magnitude number=1 K: Kukarkin --- r_mag Reference for apparent magnitude --- U-B U-B color index mag B-V B-V color index mag r_U-B Reference for color indices --- Per Period of variability d r_Per Period reference --- Binary Component designation for binaries --- Var Type of variability --- Spectral type and luminosity class No star number --- m_No Multiplicity index on No --- SpType Spectral type and luminosity class --- r_SpType Reference for spectral type --- Guide to radio emission and observation priority No Star number --- VLA Reference for VLA position --- MERLIN Reference for MERLIN position --- VLBI Reference for VLBI position --- NTR Reference for nonthermal radiation --- REC1 Reference for radio emission confirmed --- REC2 Second reference for radio emission confirmed --- REC3 Third reference for radio emission confirmed --- Other Other indication for radio emission --- r_Other Reference for Other --- Other2 Other indication for radio emission --- r_Other2 Reference for Other2 --- Hip Hipparcos Superhigh Priority Radio Star reference --- VLApro VLA programme star reference --- VLApro2 Second VLA programme star reference --- MERLINpro MERLIN programme star reference --- VLBIpro VLBI programme star reference --- References RefNo Reference Number number= Finding charts of all stars are in ref. 0163. For 1022 and 1197, they are also in ref. 95. number= 1022: X-ray source (Ref.0153) 1027: radio map in Ref.0068 1028: Complex structure of radio core and halo (Ref.0143). Radio map in Ref.0143 1128: X-ray source (Ref.0192) 1176: Member of the Sco-Cen ass.; optical data in Kudritzki and Reimers (1978A&A....70..227K); additional positions and discussion in Clauzet et al. 1990A&A...233..608C (Ref.0192), Radio map in Ref.0126 and Ref.0075. 1219: Fluctuating X-ray system (Ref.0123), the invisible companion is believed to be a black hole (Ref.0192) 2340: X-ray source (Ref.0192) 2384: Active late-type star, pre main sequence star, visual double star? 2609: Emission line star (Ref.0111) 2611: X-ray source, emission line star (Ref.0192) 2908: Naked T Tau star, X-ray source, T Tau association (Ref.0192) optical data in Walter et al. 1987ApJ...314..297W (Ref.0192) --- BibCode Bibliographical code as used in electronic journals and databases (ADS, NED, SIMBAD) number= Finding charts of all stars are in ref. 0163. For 1022 and 1197, they are also in ref. 95. number= 1022: X-ray source (Ref.0153) 1027: radio map in Ref.0068 1028: Complex structure of radio core and halo (Ref.0143). Radio map in Ref.0143 1128: X-ray source (Ref.0192) 1176: Member of the Sco-Cen ass.; optical data in Kudritzki and Reimers (1978A&A....70..227K); additional positions and discussion in Clauzet et al. 1990A&A...233..608C (Ref.0192), Radio map in Ref.0126 and Ref.0075. 1219: Fluctuating X-ray system (Ref.0123), the invisible companion is believed to be a black hole (Ref.0192) 2340: X-ray source (Ref.0192) 2384: Active late-type star, pre main sequence star, visual double star? 2609: Emission line star (Ref.0111) 2611: X-ray source, emission line star (Ref.0192) 2908: Naked T Tau star, X-ray source, T Tau association (Ref.0192) optical data in Walter et al. 1987ApJ...314..297W (Ref.0192) --- Text Text of reference number= Finding charts of all stars are in ref. 0163. For 1022 and 1197, they are also in ref. 95. number= 1022: X-ray source (Ref.0153) 1027: radio map in Ref.0068 1028: Complex structure of radio core and halo (Ref.0143). Radio map in Ref.0143 1128: X-ray source (Ref.0192) 1176: Member of the Sco-Cen ass.; optical data in Kudritzki and Reimers (1978A&A....70..227K); additional positions and discussion in Clauzet et al. 1990A&A...233..608C (Ref.0192), Radio map in Ref.0126 and Ref.0075. 1219: Fluctuating X-ray system (Ref.0123), the invisible companion is believed to be a black hole (Ref.0192) 2340: X-ray source (Ref.0192) 2384: Active late-type star, pre main sequence star, visual double star? 2609: Emission line star (Ref.0111) 2611: X-ray source, emission line star (Ref.0192) 2908: Naked T Tau star, X-ray source, T Tau association (Ref.0192) optical data in Walter et al. 1987ApJ...314..297W (Ref.0192) --- table.txt The catalog as one printable ascii file. Patricia Bauer CDS 1996 Sep 02 UNKNOWN UNKNOWN The catalogue (table.txt) has been transformed into seven tables. J_A+AS_122_529.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest. XV: P IV spectral lines. J/A+AS/122/533 J/A+AS/122/533 Stark broadening of P IV spectral lines Stark broadening of spectral lines of multicharged ions of astrophysical interest. XV: P IV spectral lines. M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 122 533 1997 1997A&AS..122..533D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines Atomic physics atomic data line: profiles Using a semiclassical approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 114 P IV multiplets for perturber densities 10^15^-10^20^cm^-3^ and temperatures T=5000-1000000K. The obtained results have been compared with results obtained by using various simpler approaches.
Stark broadening parameters due to e-, p- and He III-impacts for P IV N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ (4) --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ (4) --- dHe++ shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1996 Oct 09 Dr Milan Dimitrijevic <mdimitrijevic@aob.aob.bg.ac.yu> J_A+AS_122_533.xml Secondary standard stars for uvby-beta CCD photometry J/A+AS/122/559 J/A+AS/122/559 uvby-beta CCD photometry secondary standard Secondary standard stars for uvby-beta CCD photometry J V Clausen S S Larsen J M Garcia A Gimenez J Storm Astron. Astrophys. Suppl. Ser. 122 559 1997 1997A&AS..122..559C Photometry, standards Photometry, uvby, beta Photometry, Stroemgren astronomical data bases: miscellaneous stars: fundamental parameters stars: general Accurate standard uvby indices are presented for 73 southern B, A, F and G stars in the V magnitude range 8.2 to 10.9. They cover all three transformation regions of the uvby system (Olsen 1983A&AS...54...55O) well. Standard {beta} indices are included for the 55 B, A, and F stars in the sample. Our results provide a useful set of secondary standards for uvby {beta} CCD photometry with southern hemisphere 1-2m class telescopes. A critical comparison with published photometry, in general based on fewer observations, is given.
Catalogue of transformed uvby indices for the observed primary standard stars. HD HD (Cat. <III/135>) number --- T uvby transformation region: A (BAF),D (GKV), G (GKIII) --- o_Vmag Number of observations --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag b-y b-y color index mag e_b-y rms uncertainty on b-y mag m1 m1 color index mag e_m1 rms uncertainty on m1 mag c1 c1 color index mag e_c1 rms uncertainty on c1 mag dVmag Standard - transformed V magnitude value 10-3mag db-y Standard - transformed b-y color index value 10-3mag dm1 Standard - transformed m1 color index value 10-3mag dc1 Standard - transformed c1 color index value 10-3mag Catalogue of transformed beta indices for the observed primary standard stars. HD HD number --- T Transformation region --- o_Beta Number of observations --- Beta Beta color index mag e_Beta rms uncertainty on Beta mag dBeta Standard - transformed Beta value 10-3mag Catalogue of observed secondary standard stars HD/CPD HD or CPD name --- ID E-region identification (Cousins & Stoy 1962RGOB...49....3C), --- T uvby (A,D,G) & beta (A,B) transformation regions --- o_Vmag Number of observations in Vmag --- o_b-y Number of observations in uvby --- o_Beta Number of observations in Beta --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag b-y b-y color index mag e_b-y rms uncertainty on b-y mag m1 m1 color index mag e_m1 rms uncertainty on m1 mag c1 c1 color index mag e_c1 rms uncertainty on c1 mag Beta Beta color index mag e_Beta rms uncertainty on Beta mag Patricia Bauer CDS 1996 Sep 05 Jens Viggo Clausen <jvc@astro.ku.dk> J_A+AS_122_559.xml The ATCA/VLA OH 1612 MHz survey. I. Observations of the Galactic Bulge Region J/A+AS/122/79 J/A+AS/122/79 Galactic Bulge Region OH 1612MHz survey. I. The ATCA/VLA OH 1612 MHz survey. I. Observations of the Galactic Bulge Region M N Sevenster J M Chapman H J Habing N E B Killeen M Lindqvist Astron. Astrophys. Suppl. Ser. 122 79 1997 1997A&AS..122...79S Masers Radio lines Galaxy: center Galaxy: stellar content radio lines: stars stars: AGB and post-AGB surveys techniques: image processing We present observations of the region between |l|<=10{deg} and |b|<=3{deg} in the OH 1612.231MHz line, taken in 1993 October and November with the Australia Telescope Compact Array. The region was systematically searched for OH/IR stars and was covered completely with 539 pointing centres separated by 30'. The size of the dataset calls for a special reduction technique that is fast, reliable and minimizes the output (positions and velocities of possible stars only). Having developed such a reduction method we found 307 OH masing objects, 145 of which are new detections. Out of these, 248 have a standard double-peaked spectral profile, 55 a single-peaked profile and 4 have nonstandard or irregular profiles. In this article we analyse the data statistically and give classifications and identifications with known sources where possible. The astrophysical, kinematical, morphological and dynamical properties of subsets of the data will be addressed in future articles. These observations are part of a larger survey, covering |l|<=45{deg} and |b|<=3{deg}, with the Australia Telescope Compact Array and the Very Large Array. The electronic version of this paper, that includes table and spectra, can be obtained from http://www.ed-phys.fr.
Compact OH-maser sources No Source number --- Name Source name (based on galactic longitude and latitude) --- Type Spectrum type --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec Delta Position scatter arcsec R Offset from pointing centre arcmin VL Velocity blue-shifted peak km/s VH Velocity red-shifted peak km/s VC Velocity central star km/s VE Outflow velocity shell km/s SL Flux density blue-shifted peak Jy SH Flux density red-shifted peak Jy Rms Rms noise in empty cubes mJy Ref Number reference for previous detection --- IRAS Name of nearest IRAS point source <II/125> --- N Distance to nearest IRAS PS as fraction of IRAS error ellipse --- table1.tex LaTeX version of table1 M.N. Sevenster Sterrewacht Leiden, NL 1996 Jul 19 J_A+AS_122_79.xml Multicolour deep CCD photometric study of the moderately young southern open star clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087 J/A+AS/122/9 J/A+AS/122/9 CCD UBVRI Photometry of 4 open clusters Multicolour deep CCD photometric study of the moderately young southern open star clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087 R Sagar R D Cannon Astron. Astrophys. Suppl. Ser. 122 9 1997 1997A&AS..122....9S Clusters, open Photometry, UBVRI Hertzsprung-Russell (HR diagram) open clusters and associations: individual (NGC 3228, NGC 4103) stars: evolution CCD observations in the U, B, V, R and I passbands have been used to generate colour-colour and deep colour-magnitude diagrams for the young open star clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087. The sample consists of about 2000 stars reaching down to V=20mag. The interstellar extinction across the face of the imaged cluster regions seems to be uniform with average values of E(B-V)=0.31, 0.34 and 0.22mag for NGC 4103, NGC 5662 and NGC 6087 respectively. The distances to the clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087 have been estimated as 0.5+/-0.05, 2.0+/-0.3, 0.8+/-0.1 and 1.0+/-0.1kpc respectively, while the corresponding ages estimated from the theoretical stellar evolutionary isochrones fitted to the bright proper motion cluster members are ~100, 30, 80 and 65Myr respectively. Present data are consistent with the membership of the Cepheid variable V Cen to NGC 5662 and of S Norm to NGC 6087. Heavy contamination by foreground and background field stars has unfortunately made it impossible to reach definite conclusions about the faint luminosity function, and the data do not reach faint enough limits to investigate pre-main sequence stars.
NGC 3228 C 1019-514 10 21.8 -51 43 NGC 4103 C 1204-609 12 06.7 -61 15 NGC 5662 C 1431-563 14 35.2 -56 33 NGC 6087 C 1614-577 16 18.9 -57 54
Relative positions and UBVRI mag in NGC 3228 Relative positions and UBVRI mag in NGC 4103 Relative positions and UBVRI mag in NGC 5662 Relative positions and UBVRI mag in Regions 2 and 3 of NGC 6087 SeqNum Sequential star number --- Xpos X position pix Ypos Y position pix Vmag V magnitude mag U-B U-B colour index mag B-V B-V colour index mag V-R V-R colour index mag V-I V-I colour index mag Name Other identifications number=1 Prefixes are: W: Wesselink, 1969MNRAS.146..329W MV: Moffat & Vogt, 1973A&AS...10..135M H: Haug, 1978A&AS...34..417H K: King, 1980, J. Proc. R. Soc. N.S.W. 113, 7 C: Claria et al., 1991MNRAS.249..193C L: Landoldt, 1964ApJS....8..329L --- Relative positions and UBVRI mag in Region 1 of NGC 6087 SeqNum Sequential star number --- Xpos X position pix Ypos Y position pix Vmag V magnitude mag U-B U-B colour index mag B-V B-V colour index mag V-I V-I colour index mag Name Other identifications number=1 L: Landoldt (1964ApJS....8..329L) --- Patricia Bauer CDS 1996 Jul 24 Ram Sagar <sagar@iiap.ernet.in> J_A+AS_122_9.xml Field 3 of the Palomar-Groningen Survey. I. Variable stars at the edge of the Sagittarius dwarf galaxy J/A+AS/123/115 J/A+AS/123/115 Variables stars in Palomar-Groningen field 3 Field 3 of the Palomar-Groningen Survey. I. Variable stars at the edge of the Sagittarius dwarf galaxy Y K Ng M Schultheis Astron. Astrophys. Suppl. Ser. 123 115 1997 1997A&AS..123..115N Magnitudes, photographic Stars, variable galaxies: individual (Sagittarius dwarf) Local Group stars: AGB and post-AGB stars: carbon stars: variables: other A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.
Sagittarius dwarf galaxy 19 29 58.9 -17 40 40
Catalogue of PG3 variable stars ID Star number number=1 Variable star number, following Plaut (1971A&AS....4...75P) and Wesselink (1987) --- VarType Variable type number=2 Variable star classification, where the semiregular classification is taken from Plaut (1971A&AS....4...75P); if two classifications are given, the first is from Wesselink (1987) and the second from Plaut (1971A&AS....4...75P) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Bmag Mean photographic B_J_ magnitude number=3 The mean B_J and R_F photographic magnitudes for the RR Lyrae and the Mira are from Wesselink (1987). The photographic photometry of the semiregular variables is obtained in the study by Ng (1994) mag Rmag Mean photographic R_F_ magnitude number=3 The mean B_J and R_F photographic magnitudes for the RR Lyrae and the Mira are from Wesselink (1987). The photographic photometry of the semiregular variables is obtained in the study by Ng (1994) mag P Period d Q Quality flag number=4 Quality flag (classification and period) of variable star following Wesselink (1987); Q=0: no doubt about the determined period and classification, Q=1: classification is correct but alternative period is possible, Q=2: period determination is correct but the classification is doubtful, Q=3: both period determination and classification are unreliable --- find_pg3.ps Finding charts Patricia Bauer CDS 1997 Jan 13 Yuen Keong Ng <yuen@astrpd.pd.astro.it> J_A+AS_123_115.xml The supercluster-void network. I. The supercluster catalogue and large-scale distribution J/A+AS/123/119 J/A+AS/123/119 The supercluster-void network. I. The supercluster-void network. I. The supercluster catalogue and large-scale distribution M Einasto E Tago J Jaaniste J Einasto H Andernach Astron. Astrophys. Suppl. Ser. 123 119 1997 1997A&AS..123..119E VII/4 : Abell and Zwicky Clusters of Galaxies (Abell+ 1974) Clusters, galaxy Galaxy catalogs catalogs cosmology: observations galaxies: clusters: general large-scale structure of universe We use a compilation of redshifts of rich clusters by Andernach, Tago and Stengler-Larrea (1996, in preparation) to determine superclusters of rich clusters up to a redshift of z=0.12. Superclusters were searched for with a clustering algorithm, using a neighbourhood radius of 24h^-1^Mpc (h is the Hubble constant in units of 100km/s/Mpc). The catalogue contains 220 superclusters of rich clusters, of which 90 superclusters have been determined for the first time. Table A2 gives the supercluster number, its multiplicity, centre coordinates, a list of member clusters and identifications with the catalogue by Einasto et al. (1994MNRAS.269..301E).
Superclusters of galaxies with multiplicity k>=2 SC Supercluster number --- cflag Candidate flag number=1 c stands for supercluster candidate, i.e. a supercluster in which less than two member clusters have a redshift measured --- Nmembers Supercluster multiplicity = number of member clusters --- RAdeg Right ascension (1950) of supercluster centre deg DEdeg Declination (1950) of supercluster centre deg Dist Distance of supercluster centre from Earth Mpc ID supercluster identification --- ID_E supercluster number(s) from Einasto et al. (1994MNRAS.269..301E) --- ACO Abell-ACO number of member cluster --- n_ACO Membership flag number=2 "e" indicates a cluster with estimated redshift "-" indicates a cluster which would not be a supercluster member if one had used only clusters with measured redshifts in the search algorithm --- Patricia Bauer CDS 1996 Sep 32 UNKNOWN UNKNOWN * superseded J/MNRAS/269/301 : Superclusters and voids (Einasto+, 1994) J_A+AS_123_119.xml Spectral classifications in the near infrared of stars with composite spectra. II. Study of a sample of 180 stars. J/A+AS/123/135 J/A+AS/123/135 Spectral classifications of 180 IR stars Spectral classifications in the near infrared of stars with composite spectra. II. Study of a sample of 180 stars. N Ginestet J -M Carquillat C Jaschek M Jaschek Astron. Astrophys. Suppl. Ser. 123 135 1997 1997A&AS..123..135G MK spectral classification Spectra, infrared binaries: spectroscopic infrared: stars stars: classification A sample of 180 supposedly composite-spectrum stars has been studied on the basis of spectra obtained in the near infrared (8370-8780{AA}) at a dispersion of 33{AA}/mm. The objective was to study the cooler components of the systems. Of our sample, 120 are true composite spectra, 35 are hot spectra of types B, F and 25 are Am stars. We find a strong concentration of the cooler components of the composite spectra around G8III. In view of the difficulty of classifying composite spectra, because of the superposition of an early type dwarf and a late type giant or supergiant spectrum, we have made several tests to control the classification based upon the infrared region. Since all tests gave positive results, we conclude that our classifications can be considered as being both reliable and homogeneous.
Classifications of the cool components, SP(IR), of stars with composite spectra HD/BD HD of BD number of the star --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag --- B-V B-V color index mag SpIR This work spectral type number=1 A - or + sign following the Sp(IR) luminosity class indicates that the object is probably slightly more or less luminous. --- n_SpIR Note on the object number=2 Individual notes: HD 18715: classification based on the cool component, since both components are well separated (8") HD 26630: standard MK G0 Ib HD 51250: standard of radial velocity HD 74395: standard MK G1 Ib HD 84367: the secondary is probably an Am star HD 197177: standard MK G8 IIb HD 199378: the authors suspect the object to be composite (G5III+A) HD 209278: visual binary, separated 3.7", but the classification is based on the combined light HD 212391: the classification is based on the spectrum of the cool star since the separation of 4.3" permits to observe individually each component. --- Sp1 Spectral type --- r_Sp1 References for spectral type number=3 Abt (1977) =1977PASP...89...29A Abt (1981) =1981ApJS...45..437A Abt (1984) =1984ApJ...285..247A Abt (1985) =1985ApJS...59...95A Abt (1986) =1986ApJ...309..260A Appenzeller (1967) =1967PASP...79..102A Arellano (1986) =1986ApJ...302..767A Bahng (1958) =1958ApJ...128..572B Batten (1989) =1989PDAO...17....1B Beavers (1982) =1982ApJS...49..273B Bertaud (1970) =1970A&AS....1....7B Bidelman (1954) =1954ApJS....1..175B Bidelman (1957a) =1957PASP...69..147B Bidelman (1957b) =1957PASP...69..326B Bidelman (1958) =1958PASP...70..168B Bidelman (1988) =1988PASP..100.1084B Burki (1983) =1983A&A...124..256B Catalogue HD =Catalogue <III/135> Corbally (1984) =1984ApJS...55..657C Cowley (1969) =1969AJ.....74..375C Cowley (1971) =1971PASP...83..296C Cowley (1976) =1976PASP...88...95C Cowley (1979) =1979PASP...91...83C Edwards (1976) =1976AJ.....81..245E Evans (1979) =1979ApJ...228..497E Griffin (1976) =1976Obs....96..153G Griffin (1988) =1988JApA....9..193G Griffin (1989) =1989JApA...10..433G Griffin (1990) =1990JApA...11..281G Griffin (1992) =1992A&A...254..289G Griffin (1994) =1994MNRAS.270..409G Harlan (1974) =1974AJ.....79..682H Harmer (1983) =1983MNRAS.204..927H Heard (1956) =1956PDDO....2..105H Hendry (1978) =1978AJ.....83..615H Hendry (1981) =1981AJ.....86..271H Hoffleit (1982) =Catalogue <V/50> Houk (1982) =Catalogue <III/80> Houk (1988) =Catalogue <III/133> Hynek (1959) =1959PASP...71..310H Jaschek (1991) =1991A&A...252..229J Keenan (1989) =Catalogue <III/150> Kuhi (1963) =1963PASP...75..448K Malaroda (1973) =1973PASP...85..328M Malaroda (1975) =1975AJ.....80..637M Markowitz (1969) Ph.D thesis, Ohio State Univ. McAlister (1982) =1982AJ.....87..563M Meisel (1968) =1968AJ.....73..350M Moore (1950) =1950ApJ...112...48M Olsen (1980) =1980A&AS...39..205O Roman (1949) =1949ApJ...110..205R Sato (1990) =1990A&AS...85.1069S Slettebak (1955) =1955ApJ...121..653S Slettebak (1969) =1969AJ.....74..373S Stebbins (1956) =1956ApJ...123..440S Stephenson (1960) =1960AJ.....65...60S Stephenson (1969) =1969AJ.....74..689S Stickland (1988) =1988IUE88...2...27S Strassmeier (1990) =1990A&A...230..389S Underhiller (1990) =1990A&A...230..389S Underhill (1954) =1954AJ.....59..332U Walker (1966) =1966Obs....86..154W Wellmann (1951) =1951AN....279..257W Wright (1970) =1970VA.....12..147W --- Sp2 Spectral type --- n_Sp2 Note on the object number=2 Individual notes: HD 18715: classification based on the cool component, since both components are well separated (8") HD 26630: standard MK G0 Ib HD 51250: standard of radial velocity HD 74395: standard MK G1 Ib HD 84367: the secondary is probably an Am star HD 197177: standard MK G8 IIb HD 199378: the authors suspect the object to be composite (G5III+A) HD 209278: visual binary, separated 3.7", but the classification is based on the combined light HD 212391: the classification is based on the spectrum of the cool star since the separation of 4.3" permits to observe individually each component. --- r_Sp2 References for spectral type number=3 Abt (1977) =1977PASP...89...29A Abt (1981) =1981ApJS...45..437A Abt (1984) =1984ApJ...285..247A Abt (1985) =1985ApJS...59...95A Abt (1986) =1986ApJ...309..260A Appenzeller (1967) =1967PASP...79..102A Arellano (1986) =1986ApJ...302..767A Bahng (1958) =1958ApJ...128..572B Batten (1989) =1989PDAO...17....1B Beavers (1982) =1982ApJS...49..273B Bertaud (1970) =1970A&AS....1....7B Bidelman (1954) =1954ApJS....1..175B Bidelman (1957a) =1957PASP...69..147B Bidelman (1957b) =1957PASP...69..326B Bidelman (1958) =1958PASP...70..168B Bidelman (1988) =1988PASP..100.1084B Burki (1983) =1983A&A...124..256B Catalogue HD =Catalogue <III/135> Corbally (1984) =1984ApJS...55..657C Cowley (1969) =1969AJ.....74..375C Cowley (1971) =1971PASP...83..296C Cowley (1976) =1976PASP...88...95C Cowley (1979) =1979PASP...91...83C Edwards (1976) =1976AJ.....81..245E Evans (1979) =1979ApJ...228..497E Griffin (1976) =1976Obs....96..153G Griffin (1988) =1988JApA....9..193G Griffin (1989) =1989JApA...10..433G Griffin (1990) =1990JApA...11..281G Griffin (1992) =1992A&A...254..289G Griffin (1994) =1994MNRAS.270..409G Harlan (1974) =1974AJ.....79..682H Harmer (1983) =1983MNRAS.204..927H Heard (1956) =1956PDDO....2..105H Hendry (1978) =1978AJ.....83..615H Hendry (1981) =1981AJ.....86..271H Hoffleit (1982) =Catalogue <V/50> Houk (1982) =Catalogue <III/80> Houk (1988) =Catalogue <III/133> Hynek (1959) =1959PASP...71..310H Jaschek (1991) =1991A&A...252..229J Keenan (1989) =Catalogue <III/150> Kuhi (1963) =1963PASP...75..448K Malaroda (1973) =1973PASP...85..328M Malaroda (1975) =1975AJ.....80..637M Markowitz (1969) Ph.D thesis, Ohio State Univ. McAlister (1982) =1982AJ.....87..563M Meisel (1968) =1968AJ.....73..350M Moore (1950) =1950ApJ...112...48M Olsen (1980) =1980A&AS...39..205O Roman (1949) =1949ApJ...110..205R Sato (1990) =1990A&AS...85.1069S Slettebak (1955) =1955ApJ...121..653S Slettebak (1969) =1969AJ.....74..373S Stebbins (1956) =1956ApJ...123..440S Stephenson (1960) =1960AJ.....65...60S Stephenson (1969) =1969AJ.....74..689S Stickland (1988) =1988IUE88...2...27S Strassmeier (1990) =1990A&A...230..389S Underhiller (1990) =1990A&A...230..389S Underhill (1954) =1954AJ.....59..332U Walker (1966) =1966Obs....86..154W Wellmann (1951) =1951AN....279..257W Wright (1970) =1970VA.....12..147W --- Sp3 Spectral type --- r_Sp3 References for spectral type number=3 Abt (1977) =1977PASP...89...29A Abt (1981) =1981ApJS...45..437A Abt (1984) =1984ApJ...285..247A Abt (1985) =1985ApJS...59...95A Abt (1986) =1986ApJ...309..260A Appenzeller (1967) =1967PASP...79..102A Arellano (1986) =1986ApJ...302..767A Bahng (1958) =1958ApJ...128..572B Batten (1989) =1989PDAO...17....1B Beavers (1982) =1982ApJS...49..273B Bertaud (1970) =1970A&AS....1....7B Bidelman (1954) =1954ApJS....1..175B Bidelman (1957a) =1957PASP...69..147B Bidelman (1957b) =1957PASP...69..326B Bidelman (1958) =1958PASP...70..168B Bidelman (1988) =1988PASP..100.1084B Burki (1983) =1983A&A...124..256B Catalogue HD =Catalogue <III/135> Corbally (1984) =1984ApJS...55..657C Cowley (1969) =1969AJ.....74..375C Cowley (1971) =1971PASP...83..296C Cowley (1976) =1976PASP...88...95C Cowley (1979) =1979PASP...91...83C Edwards (1976) =1976AJ.....81..245E Evans (1979) =1979ApJ...228..497E Griffin (1976) =1976Obs....96..153G Griffin (1988) =1988JApA....9..193G Griffin (1989) =1989JApA...10..433G Griffin (1990) =1990JApA...11..281G Griffin (1992) =1992A&A...254..289G Griffin (1994) =1994MNRAS.270..409G Harlan (1974) =1974AJ.....79..682H Harmer (1983) =1983MNRAS.204..927H Heard (1956) =1956PDDO....2..105H Hendry (1978) =1978AJ.....83..615H Hendry (1981) =1981AJ.....86..271H Hoffleit (1982) =Catalogue <V/50> Houk (1982) =Catalogue <III/80> Houk (1988) =Catalogue <III/133> Hynek (1959) =1959PASP...71..310H Jaschek (1991) =1991A&A...252..229J Keenan (1989) =Catalogue <III/150> Kuhi (1963) =1963PASP...75..448K Malaroda (1973) =1973PASP...85..328M Malaroda (1975) =1975AJ.....80..637M Markowitz (1969) Ph.D thesis, Ohio State Univ. McAlister (1982) =1982AJ.....87..563M Meisel (1968) =1968AJ.....73..350M Moore (1950) =1950ApJ...112...48M Olsen (1980) =1980A&AS...39..205O Roman (1949) =1949ApJ...110..205R Sato (1990) =1990A&AS...85.1069S Slettebak (1955) =1955ApJ...121..653S Slettebak (1969) =1969AJ.....74..373S Stebbins (1956) =1956ApJ...123..440S Stephenson (1960) =1960AJ.....65...60S Stephenson (1969) =1969AJ.....74..689S Stickland (1988) =1988IUE88...2...27S Strassmeier (1990) =1990A&A...230..389S Underhiller (1990) =1990A&A...230..389S Underhill (1954) =1954AJ.....59..332U Walker (1966) =1966Obs....86..154W Wellmann (1951) =1951AN....279..257W Wright (1970) =1970VA.....12..147W --- Sp4 Spectral type --- r_Sp4 References for spectral type number=3 Abt (1977) =1977PASP...89...29A Abt (1981) =1981ApJS...45..437A Abt (1984) =1984ApJ...285..247A Abt (1985) =1985ApJS...59...95A Abt (1986) =1986ApJ...309..260A Appenzeller (1967) =1967PASP...79..102A Arellano (1986) =1986ApJ...302..767A Bahng (1958) =1958ApJ...128..572B Batten (1989) =1989PDAO...17....1B Beavers (1982) =1982ApJS...49..273B Bertaud (1970) =1970A&AS....1....7B Bidelman (1954) =1954ApJS....1..175B Bidelman (1957a) =1957PASP...69..147B Bidelman (1957b) =1957PASP...69..326B Bidelman (1958) =1958PASP...70..168B Bidelman (1988) =1988PASP..100.1084B Burki (1983) =1983A&A...124..256B Catalogue HD =Catalogue <III/135> Corbally (1984) =1984ApJS...55..657C Cowley (1969) =1969AJ.....74..375C Cowley (1971) =1971PASP...83..296C Cowley (1976) =1976PASP...88...95C Cowley (1979) =1979PASP...91...83C Edwards (1976) =1976AJ.....81..245E Evans (1979) =1979ApJ...228..497E Griffin (1976) =1976Obs....96..153G Griffin (1988) =1988JApA....9..193G Griffin (1989) =1989JApA...10..433G Griffin (1990) =1990JApA...11..281G Griffin (1992) =1992A&A...254..289G Griffin (1994) =1994MNRAS.270..409G Harlan (1974) =1974AJ.....79..682H Harmer (1983) =1983MNRAS.204..927H Heard (1956) =1956PDDO....2..105H Hendry (1978) =1978AJ.....83..615H Hendry (1981) =1981AJ.....86..271H Hoffleit (1982) =Catalogue <V/50> Houk (1982) =Catalogue <III/80> Houk (1988) =Catalogue <III/133> Hynek (1959) =1959PASP...71..310H Jaschek (1991) =1991A&A...252..229J Keenan (1989) =Catalogue <III/150> Kuhi (1963) =1963PASP...75..448K Malaroda (1973) =1973PASP...85..328M Malaroda (1975) =1975AJ.....80..637M Markowitz (1969) Ph.D thesis, Ohio State Univ. McAlister (1982) =1982AJ.....87..563M Meisel (1968) =1968AJ.....73..350M Moore (1950) =1950ApJ...112...48M Olsen (1980) =1980A&AS...39..205O Roman (1949) =1949ApJ...110..205R Sato (1990) =1990A&AS...85.1069S Slettebak (1955) =1955ApJ...121..653S Slettebak (1969) =1969AJ.....74..373S Stebbins (1956) =1956ApJ...123..440S Stephenson (1960) =1960AJ.....65...60S Stephenson (1969) =1969AJ.....74..689S Stickland (1988) =1988IUE88...2...27S Strassmeier (1990) =1990A&A...230..389S Underhiller (1990) =1990A&A...230..389S Underhill (1954) =1954AJ.....59..332U Walker (1966) =1966Obs....86..154W Wellmann (1951) =1951AN....279..257W Wright (1970) =1970VA.....12..147W --- Sp5 Spectral type --- r_Sp5 References for spectral type number=3 Abt (1977) =1977PASP...89...29A Abt (1981) =1981ApJS...45..437A Abt (1984) =1984ApJ...285..247A Abt (1985) =1985ApJS...59...95A Abt (1986) =1986ApJ...309..260A Appenzeller (1967) =1967PASP...79..102A Arellano (1986) =1986ApJ...302..767A Bahng (1958) =1958ApJ...128..572B Batten (1989) =1989PDAO...17....1B Beavers (1982) =1982ApJS...49..273B Bertaud (1970) =1970A&AS....1....7B Bidelman (1954) =1954ApJS....1..175B Bidelman (1957a) =1957PASP...69..147B Bidelman (1957b) =1957PASP...69..326B Bidelman (1958) =1958PASP...70..168B Bidelman (1988) =1988PASP..100.1084B Burki (1983) =1983A&A...124..256B Catalogue HD =Catalogue <III/135> Corbally (1984) =1984ApJS...55..657C Cowley (1969) =1969AJ.....74..375C Cowley (1971) =1971PASP...83..296C Cowley (1976) =1976PASP...88...95C Cowley (1979) =1979PASP...91...83C Edwards (1976) =1976AJ.....81..245E Evans (1979) =1979ApJ...228..497E Griffin (1976) =1976Obs....96..153G Griffin (1988) =1988JApA....9..193G Griffin (1989) =1989JApA...10..433G Griffin (1990) =1990JApA...11..281G Griffin (1992) =1992A&A...254..289G Griffin (1994) =1994MNRAS.270..409G Harlan (1974) =1974AJ.....79..682H Harmer (1983) =1983MNRAS.204..927H Heard (1956) =1956PDDO....2..105H Hendry (1978) =1978AJ.....83..615H Hendry (1981) =1981AJ.....86..271H Hoffleit (1982) =Catalogue <V/50> Houk (1982) =Catalogue <III/80> Houk (1988) =Catalogue <III/133> Hynek (1959) =1959PASP...71..310H Jaschek (1991) =1991A&A...252..229J Keenan (1989) =Catalogue <III/150> Kuhi (1963) =1963PASP...75..448K Malaroda (1973) =1973PASP...85..328M Malaroda (1975) =1975AJ.....80..637M Markowitz (1969) Ph.D thesis, Ohio State Univ. McAlister (1982) =1982AJ.....87..563M Meisel (1968) =1968AJ.....73..350M Moore (1950) =1950ApJ...112...48M Olsen (1980) =1980A&AS...39..205O Roman (1949) =1949ApJ...110..205R Sato (1990) =1990A&AS...85.1069S Slettebak (1955) =1955ApJ...121..653S Slettebak (1969) =1969AJ.....74..373S Stebbins (1956) =1956ApJ...123..440S Stephenson (1960) =1960AJ.....65...60S Stephenson (1969) =1969AJ.....74..689S Stickland (1988) =1988IUE88...2...27S Strassmeier (1990) =1990A&A...230..389S Underhiller (1990) =1990A&A...230..389S Underhill (1954) =1954AJ.....59..332U Walker (1966) =1966Obs....86..154W Wellmann (1951) =1951AN....279..257W Wright (1970) =1970VA.....12..147W --- Sp6 Spectral type --- r_Sp6 References for spectral type number=3 Abt (1977) =1977PASP...89...29A Abt (1981) =1981ApJS...45..437A Abt (1984) =1984ApJ...285..247A Abt (1985) =1985ApJS...59...95A Abt (1986) =1986ApJ...309..260A Appenzeller (1967) =1967PASP...79..102A Arellano (1986) =1986ApJ...302..767A Bahng (1958) =1958ApJ...128..572B Batten (1989) =1989PDAO...17....1B Beavers (1982) =1982ApJS...49..273B Bertaud (1970) =1970A&AS....1....7B Bidelman (1954) =1954ApJS....1..175B Bidelman (1957a) =1957PASP...69..147B Bidelman (1957b) =1957PASP...69..326B Bidelman (1958) =1958PASP...70..168B Bidelman (1988) =1988PASP..100.1084B Burki (1983) =1983A&A...124..256B Catalogue HD =Catalogue <III/135> Corbally (1984) =1984ApJS...55..657C Cowley (1969) =1969AJ.....74..375C Cowley (1971) =1971PASP...83..296C Cowley (1976) =1976PASP...88...95C Cowley (1979) =1979PASP...91...83C Edwards (1976) =1976AJ.....81..245E Evans (1979) =1979ApJ...228..497E Griffin (1976) =1976Obs....96..153G Griffin (1988) =1988JApA....9..193G Griffin (1989) =1989JApA...10..433G Griffin (1990) =1990JApA...11..281G Griffin (1992) =1992A&A...254..289G Griffin (1994) =1994MNRAS.270..409G Harlan (1974) =1974AJ.....79..682H Harmer (1983) =1983MNRAS.204..927H Heard (1956) =1956PDDO....2..105H Hendry (1978) =1978AJ.....83..615H Hendry (1981) =1981AJ.....86..271H Hoffleit (1982) =Catalogue <V/50> Houk (1982) =Catalogue <III/80> Houk (1988) =Catalogue <III/133> Hynek (1959) =1959PASP...71..310H Jaschek (1991) =1991A&A...252..229J Keenan (1989) =Catalogue <III/150> Kuhi (1963) =1963PASP...75..448K Malaroda (1973) =1973PASP...85..328M Malaroda (1975) =1975AJ.....80..637M Markowitz (1969) Ph.D thesis, Ohio State Univ. McAlister (1982) =1982AJ.....87..563M Meisel (1968) =1968AJ.....73..350M Moore (1950) =1950ApJ...112...48M Olsen (1980) =1980A&AS...39..205O Roman (1949) =1949ApJ...110..205R Sato (1990) =1990A&AS...85.1069S Slettebak (1955) =1955ApJ...121..653S Slettebak (1969) =1969AJ.....74..373S Stebbins (1956) =1956ApJ...123..440S Stephenson (1960) =1960AJ.....65...60S Stephenson (1969) =1969AJ.....74..689S Stickland (1988) =1988IUE88...2...27S Strassmeier (1990) =1990A&A...230..389S Underhiller (1990) =1990A&A...230..389S Underhill (1954) =1954AJ.....59..332U Walker (1966) =1966Obs....86..154W Wellmann (1951) =1951AN....279..257W Wright (1970) =1970VA.....12..147W --- Stars of the sample which exhibit a hot spectrum HD/BD HD or BD name --- Vmag Vmangitude mag u_Vmag Uncertainty flag on Vmag --- B-V B- V color index mag Sp Spectral type --- n_Sp * when individual note number=1 HD 14262: also classed A7V (Palmer et al., 1968RGOB..135..385P) HD 16646: F4Vwl (Abt, 1984ApJ...285..247A) HD 24346: slightly weak-lined F type star (Bidelman, 1988PASP..100.1084B) HD 41724: Am (Bidelman, 1988PASP..100.1084B; Carquillat et al., 1988A&AS...75..305C) HD 48953: G5Ia+A5V (Markowitz, 1969, Ph.D thesis, Ohio State Univ.), Ap Sr-Eu (Bidelman, 1988PASP..100.1084B) HD 51565: G2IIIe (Kuhi, 1963PASP...75..448K); Am (Smith, 1973ApJS...25..277S) HD 60178: Castor B HD 68119: larger proper motion (CDS); moderatly weak-lines F type star (Bidelman, 1988PASP..100.1084B) HD 76369: appears normal (Bidelman, 1988PASP..100.1084B) HD 76370: G5III+A0V (Markovitz, 1969, Ph.D thesis, Ohio State Univ.) HD 83270: Am (Bidelman, 1988PASP..100.1084B; Ginestet et al., 1991A&AS...91..265G) HD 83808: SB2. The dominating spectrum is that of an Am star, the secondary could be a late F type. Also classified A1V+F6II (Markovitz, 1969, Ph.D thesis, Ohio State Univ.) and A5V+F8III (Parsons, 1983ApJS...53..553P) HD 86167: Am (Abt, 1984ApJ...285..247A) HD 88923: F2Vwl (Abt, 1984ApJ...285..247A) HD 91172: Fm Delta Del (Houk & Smoth-Moore, 1988 Catalogue <III/133>) HD 97336: Bidelman (1988PASP..100.1084B): "not composite" HD 107054: A8V (Palmer et al., 1968RGOB..135..385P); A9IVn (Gray & Garrison, 1989ApJS...69..301G) HD 114519: RS CVn (SB2), Algol eclipsing type binary; Batten et al (19899PDAO...17....1B): F4IV-V+K0IV; Strassmeier & Fekel (1990A&A...230..389S): F6IV+G8IV. The spectrum is difficult to classify because of the high rotation, but the Ti/Fe ratios suggest a secondary at least as late as K4. HD 120544: F7V (Cowley, 1976PASP...88...95C) HD 123102: A9IV (Abt, 1981ApJS...45..437A); visual double, sep. 13.5" HD 187949: A1V+F4III: (Markowitz, 1969Ph.D thesis, Ohio State Univ.); Algol type eclipsing binary. HD 206088: F0p Sr (Bertaud, 1959JO.....42...45B) HD 208132: Am (Bertaud, 1965JO.....48..211B) HD 209790: Am (Slettebak, 1963ApJ...138..118S) HD 209791: F7V (Slettebak, 1963ApJ...138..118S) HD 214605: Am (Bidelman, 1988PASP..100.1084B) HD 239746: B2V comp.? (Niedzielski & Muciek, 1988AcA....38..225N) HD 239933: is not in the CDS database --- SpIR This work spectral type --- n_SpIR * when individual note number=1 HD 14262: also classed A7V (Palmer et al., 1968RGOB..135..385P) HD 16646: F4Vwl (Abt, 1984ApJ...285..247A) HD 24346: slightly weak-lined F type star (Bidelman, 1988PASP..100.1084B) HD 41724: Am (Bidelman, 1988PASP..100.1084B; Carquillat et al., 1988A&AS...75..305C) HD 48953: G5Ia+A5V (Markowitz, 1969, Ph.D thesis, Ohio State Univ.), Ap Sr-Eu (Bidelman, 1988PASP..100.1084B) HD 51565: G2IIIe (Kuhi, 1963PASP...75..448K); Am (Smith, 1973ApJS...25..277S) HD 60178: Castor B HD 68119: larger proper motion (CDS); moderatly weak-lines F type star (Bidelman, 1988PASP..100.1084B) HD 76369: appears normal (Bidelman, 1988PASP..100.1084B) HD 76370: G5III+A0V (Markovitz, 1969, Ph.D thesis, Ohio State Univ.) HD 83270: Am (Bidelman, 1988PASP..100.1084B; Ginestet et al., 1991A&AS...91..265G) HD 83808: SB2. The dominating spectrum is that of an Am star, the secondary could be a late F type. Also classified A1V+F6II (Markovitz, 1969, Ph.D thesis, Ohio State Univ.) and A5V+F8III (Parsons, 1983ApJS...53..553P) HD 86167: Am (Abt, 1984ApJ...285..247A) HD 88923: F2Vwl (Abt, 1984ApJ...285..247A) HD 91172: Fm Delta Del (Houk & Smoth-Moore, 1988 Catalogue <III/133>) HD 97336: Bidelman (1988PASP..100.1084B): "not composite" HD 107054: A8V (Palmer et al., 1968RGOB..135..385P); A9IVn (Gray & Garrison, 1989ApJS...69..301G) HD 114519: RS CVn (SB2), Algol eclipsing type binary; Batten et al (19899PDAO...17....1B): F4IV-V+K0IV; Strassmeier & Fekel (1990A&A...230..389S): F6IV+G8IV. The spectrum is difficult to classify because of the high rotation, but the Ti/Fe ratios suggest a secondary at least as late as K4. HD 120544: F7V (Cowley, 1976PASP...88...95C) HD 123102: A9IV (Abt, 1981ApJS...45..437A); visual double, sep. 13.5" HD 187949: A1V+F4III: (Markowitz, 1969Ph.D thesis, Ohio State Univ.); Algol type eclipsing binary. HD 206088: F0p Sr (Bertaud, 1959JO.....42...45B) HD 208132: Am (Bertaud, 1965JO.....48..211B) HD 209790: Am (Slettebak, 1963ApJ...138..118S) HD 209791: F7V (Slettebak, 1963ApJ...138..118S) HD 214605: Am (Bidelman, 1988PASP..100.1084B) HD 239746: B2V comp.? (Niedzielski & Muciek, 1988AcA....38..225N) HD 239933: is not in the CDS database --- Patricia Bauer CDS 1996 Sep 27 J_A+AS_123_135.xml Atomic data from the IRON Project. XXII. Radiative rates for the forbidden transitions within the ground configuration of ions in the Carbon and Oxygen isoelectronic sequences. J/A+AS/123/159 J/A+AS/123/159 IRON Project. XXII. C and O radiative rates Atomic data from the IRON Project. XXII. Radiative rates for the forbidden transitions within the ground configuration of ions in the Carbon and Oxygen isoelectronic sequences. M E Galavis C Mendoza C J Zeippen Astron. Astrophys. Suppl. Ser. 123 159 1997 1997A&AS..123..159G J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths 1997A&AS..122..167B : IRON Project XX. Fe I oscillator strengths 1997A&AS..122..177P : IRON Project XXI. Fe I fine-structure transition Atomic physics atomic data atomic processes The transition probabilities (s-1) within the ground configuration calculated in the present work for ions belonging to the carbon isoelectronic sequence are listed in Table 5, while those for ions belonging to the oxygen sequence are listed in Table 7. The first column in either table corresponds to the ion atomic number (Z), the second to the levels between which the transition occurs (Trans.), the third to the electric quadrupole transition probability (E2) and the last to the magnetic dipole transition probability (M1).
Transition probabilities within the ground configuration of the carbon sequence Transition probabilities within the ground configuration of the oxygen sequence Z Atomic number --- Trans. Levels between which transitions occur --- E2 Electric quadrupole transition probability s-1 M1 Magnetic dipolar transition probability s-1 Patricia Bauer CDS 1996 Nov 15 Martha Elena Galavis <mgalavis@hera.ivic.ve> J_A+AS_123_159.xml Four clour photometry of late-type binary systems. I. First uvby{beta} light curves of ZZ Ursae Majoris. J/A+AS/123/1 J/A+AS/123/1 uvbyBeta photometry of ZZ UMa Four clour photometry of late-type binary systems. I. First uvby{beta} light curves of ZZ Ursae Majoris. R Clement M Garcia V Reglero J V Clausen A Bravo J Suso J Fabregat J M Torrejon P Reig A Marco Astron. Astrophys. Suppl. Ser. 123 1 1997 1997A&AS..123....1C J/A+AS/123/59 : uvby photometry of BH Vir (Clement+ 1997) Binaries, eclipsing Photometry, uvby, beta binaries: eclipsing stars: fundamental parameters stars: individual (ZZ Uma) stars: late-type This paper presents first complete uvby light curves of the late-type detached eclipsing binary ZZ UMa (G0V + G8V, P=2.2993d). This binary system has been observed during eight campaigns at the Calar Alto Observatory (Almeria, Spain) and at the Sierra Nevada Observatory (Granada, Spain). 294 points distributed over the binary period and covering both eclipses are given. The comparison stars used to calculate the differential light curves (SAO 15242 and SAO 15251) were confirmed as being good reference stars with constant flux. These observations are part of a 6 year uvby and H{beta} monitoring program of low mass eclipsing binaries whose main objective is to provide accurate absolute astrophysical parameters for late-type main sequence stars. Details about the standardisation process and accuracy of the photometry are also given. The internal accuracy of the standard photometry measured as the mean RMS of the differences between standard and observed values for the standard stars observed along the program is only a few millimagnitudes. Detailed analysis of ZZ UMa, based on these light curves, will be published separately (Clement et al., 1997, Cat. <J/A+AS/123/59>).
ZZ UMa BD+62 1132 10 30 03.0 +61 48 41 SAO 15242 BD+62 1138 10 38 10.0 +61 46 27
Standard stars used in the program campaigns Campaign Order number of one or more of the 16 campaigns carried out inside the observational program, in which the standard star was observed --- No Total number of measurements --- Name Star name --- ymag y magnitude mag e_ymag rms uncertainty on ymag mmag b-y b-y color index mag e_b-y rms uncertainty on b-y mmag m1 m1 color index mag e_m1 rms uncertainty on m1 mmag c1 c1 color index mag e_c1 rms uncertainty on c1 mmag beta Hbeta color index mag e_beta rms uncertainty on beta mmag dymag Standard minus observed values in y number=1 RMS dispersion and averaged values: -------------------------------------------- dy db-y dm1 dc1 dbeta -------------------------------------------- mean 0.000 0.000 0.000 0.000 0.000 RMS 0.010 0.005 0.005 0.006 0.005 -------------------------------------------- mag db-y Standard minus observed values in b-y number=1 RMS dispersion and averaged values: -------------------------------------------- dy db-y dm1 dc1 dbeta -------------------------------------------- mean 0.000 0.000 0.000 0.000 0.000 RMS 0.010 0.005 0.005 0.006 0.005 -------------------------------------------- mag dm1 Standard minus observed values in m1 number=1 RMS dispersion and averaged values: -------------------------------------------- dy db-y dm1 dc1 dbeta -------------------------------------------- mean 0.000 0.000 0.000 0.000 0.000 RMS 0.010 0.005 0.005 0.006 0.005 -------------------------------------------- mag dc1 Standard minus observed values in c1 number=1 RMS dispersion and averaged values: -------------------------------------------- dy db-y dm1 dc1 dbeta -------------------------------------------- mean 0.000 0.000 0.000 0.000 0.000 RMS 0.010 0.005 0.005 0.006 0.005 -------------------------------------------- mag dbeta Standard minus observed values in Hbeta number=1 RMS dispersion and averaged values: -------------------------------------------- dy db-y dm1 dc1 dbeta -------------------------------------------- mean 0.000 0.000 0.000 0.000 0.000 RMS 0.010 0.005 0.005 0.006 0.005 -------------------------------------------- mag Differential magnitudes (ZZ UMa - SAO 15242) HJD Heliocentric Julian day d Dumag Differential u magnitude mag Dvmag Differential v magnitude mag Dbmag Differential b magnitude mag Dymag Differential y magnitude mag fig1.ps ZZ UMa differential light curve. y filter table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 Patricia Bauer CDS 1996 Sep 29 J_A+AS_123_1.xml A new radial velocity curve for the RS Canum Venatoricorum star Sigma Geminorum. Constraints on its physical parameters. J/A+AS/123/209 J/A+AS/123/209 Radial velocity curve of Sigma Gem A new radial velocity curve for the RS Canum Venatoricorum star Sigma Geminorum. Constraints on its physical parameters. R Duemmler I V Ilyin I Tuominen Astron. Astrophys. Suppl. Ser. 123 209 1997 1997A&AS..123..209D Binaries, spectroscopic Radial velocities Stars, variable Stars, variable binaries: spectroscopic stars: fundamental parameters stars: individual (sigma Gem) The table contains the radial velocities of the RS CVn star sigma Geminorum measured by cross-correlation using Beta Oph as template from the high-resolution SOFIN spectra around 6175A.
sigma Gem HD 62044 HR 2973 07 43 18.4 +28 53 12
Radial velocities measured from the SOFIN spectra OBSdate civil date of observation "DD/MM/YY" HJD Heliocentric Julian Date of mid-exposure d RV heliocentric radial velocity km/s Patricia Bauer CDS 1996 Sep 26 Rolf Duemmler <duemmler@gstar.Helsinki.FI> J_A+AS_123_209.xml The B3-VLA quasar sample J/A+AS/123/219 J/A+AS/123/219 The B3-VLA Quasar Sample The B3-VLA quasar sample M Vigotti G Vettolani R Merighi J Lahulla M Pedani Astron. Astrophys. Suppl. Ser. 123 219 1997 1997A&AS..123..219V QSOs Redshifts galaxies: active quasars: general radio continuum: general A new low frequency radio selected Sample of 125 Quasars complete down to 100mJy at 408MHz is presented in this paper. The sample is a part of the B3-VLA sample: 1050 radiosources selected from the B3 catalogue at 408MHz and observed at the VLA (1465MHz, C and A configurations). Out of the 352 sources, identified on the POSS-I down to m_r_~20.0, 172 are quasar candidates. In this paper we give the final assessment of the quasar sample from spectroscopic observations of the candidates. The final complete quasar sample consists of 125 objects. Furthermore 3 Bl Lac objects have been identified and two Bl Lac candidates.
The B3-VLA Quasars Complete Sample Sample Sample number --- B3 B3 name --- m_B3 Multiplicity index on B3 --- RAh Rigth ascension (B1950) h RAm Rigth ascension (B1950) min RAs Rigth ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec F408MHz Flux at 408MHz Jy Alpha Spectral index. See Note number=1 Flux proportional to : nu ** (- alpha) --- Redmag Red Magnitude --- z Redshift (blank=unknown) --- Ref. References (see ref file) --- Lines identifications and Redshifts B3 B3 name --- m_B3 Multiplicity index on B3 --- ID Original identification number=1 B: Blue starlike objects N: Red or Neutral color objects G: galaxy --- Line Spectral line --- l_LamObs Limit flag on LamObs --- LamObs Observed wavelength 0.1nm LamRest Rest wavelength 0.1nm zline Line redshift --- NewId New identification. --- z Average redshift --- e_z Redshift uncertainty --- Quasar Candidates with Different Spectroscopic Identification. B3 B3 name --- m_B3 Multiplicity index on B3 --- ID Original identification --- Redmag Red magnitude --- IDnew New identification --- Ref References (see ref file) --- References Ref Reference code --- BibCode BibCode --- Cat CDS catalogue number or priv. comm. --- fig1.ps Distribution of the radio-optical displacements for 57 unresolved quasars fig2.ps B3 magnitudes versus APM magnitudes fig3.ps Magnitudes distributions for different B3-VLA flux interval and 3CR sample fig4.ps Some representative spectra for the quasars in the B3-VLA sample fig6.ps Redshift distribution for the quasars in the B3-VLA sample Patricia Bauer CDS 1997 May 23 Marco Pedani <PEDANI@astbo1.bo.cnr.it> J_A+AS_123_219.xml Illumination in binaries J/A+AS/123/273 J/A+AS/123/273 Illumination in binaries Illumination in binaries J M Hameury H Ritter Astron. Astrophys. Suppl. Ser. 123 273 1997 1997A&AS..123..273H Accretion accretion, accretion disks binaries: close methods: numerical X-rays: stars We give a simple, but accurate method that can be used to account for illumination in compact binary systems which have a low-mass companion, even if spherically symmetric illumination of the secondary star (not necessarily on the main sequence) is not assumed. This is done by introducing a multiplicative factor {PHI} in the Stefan-Boltzmann surface boundary condition, which accounts for the blocking of the intrinsic secondary flux by X-ray heating of the photospheric layers. Numerical fits and tables for {PHI} are given for unperturbed effective temperatures in the range 2500-5600K and logg in the range 1.0-5.0.
Function G(x) logg Surface gravity cm/s2 log(Teff) Effective temperature of the unilluminated star K log(1+x) log(1+x) where x is the illuminating flux in units of the unperturbed stellar flux --- -log(G(x)) log(G(x)) where G is the fraction of the interior flux that is not blocked by illumination --- Coefficients of the fit of the modified Stefan-Boltzmann surface boundary condition. R2/a Ratio of the secondary radius versus orbital separation (f2=R2/a) --- logg Surface gravity cm/s2 log(Teff) Effective temperature of the unilluminated star K a1 Coefficient a1 of the polynomial fit of the modified boundary condition --- a2 Coefficient a2 of the polynomial fit of the modified boundary condition --- a3 Coefficient a3 of the polynomial fit of the modified boundary condition --- Patricia Bauer CDS 1996 Sep 24 Jean Marie Hameury <hameury@cdsxb9.u-strasbg.fr> J_A+AS_123_273.xml New "weak-line" T Tauri stars in Lupus J/A+AS/123/329 J/A+AS/123/329 New weak-line T Tauri stars in Lupus New "weak-line" T Tauri stars in Lupus J Krautter R Wichmann J H M M Schmitt J M Alcala R Neuhaeuser L Terranegra Astron. Astrophys. Suppl. Ser. 123 329 1997 1997A&AS..123..329K IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) IX/11 : ROSAT Source Catalog (Voges+ 1994) J/A+A/320/185 : T Tauri UBVRIcJHKL photometry (Wichmann+ 1997) Wichmann R., Krautter J., Covino E., Alcala J.M., Neuhaeuser R., Schmitt J.H.M.M., 1997A&A...320..185W Stars, pre-main sequence X-ray sources ISM: individual (Lupus clouds) stars: formation stars: pre-main sequence surveys X-rays: stars We present first results obtained by a survey of the Lupus star forming region in search of new T Tauri stars. This study has been performed on the basis of deep pointed ROSAT observations in the Lupus dark clouds as well as data from the ROSAT All-Sky-Survey in the surrounding, less obscured regions. Our survey covers an area of about 230 square degrees, located between 15^h^6^m^ and 16^h^24^m^ in right ascension and between -47^o^ and -32^o^ in declination. Identification of ROSAT All-Sky-Survey sources in this area by means of optical spectroscopy revealed 89 T Tauri stars, 86 of them "weak-line" T Tauri stars (WTTS not known from previous studies of this region. Our pointed ROSAT observations led to the identification of 47 more T Tauri stars, giving a total of 136 new T Tauri stars. The large area of our study, as compared with previous works, allows us to study the spatial distribution of WTTS in this star forming region on alarge scale. We find the new WTTS to be distributed over the whole area of our survey, indicating that their spatial distribution might extend well beyond our study area. Contrary to the Lupus T Tauri stars known prior to this study, the WTTS discovered by the ROSAT All-Sky-Survey are not clustered in the regions of highest extinction, i.e. the dark clouds.
ROSAT
New T Tauri stars in Taurus-Auriga No Sequential number --- Star Identifier of star --- NA Note on X-ray discovery number=1 Stars marked with '1', '2', or '3' have been discovered by pointed observations in the Lupus 1, Lupus 2 or Lupus 3 clouds, respectively. Left blank for stars discovered by the ROSAT All-Sky Survey. --- RAh Right Ascension for equinox 2000.0 number=2 If declination is given with one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. h RAm Right Ascension for equinox 2000.0 number=2 If declination is given with one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. min RAs Right Ascension for equinox 2000.0 number=2 If declination is given with one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. s DE- Declination sign --- DEd Declination for equinox 2000.0 number=2 If declination is given with one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. deg DEm Declination for equinox 2000.0 number=2 If declination is given with one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. arcmin DEs Declination for equinox 2000.0 number=2 If declination is given with one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. arcsec EWHa Equivalent width for H_alpha 0.1nm SpT Spectral type --- Vmag V magnitude number=3 Magnitudes given with two decimals are from our own measurements (Wichmann et al. 1997A&A...320..185W), those given with one decimal only are taken from the GSC. A value of zero means that no magnitude is available. mag New Non-TTS emission-line objects in Lupus No Sequential number --- Star Identifier of star --- NA Note on X-ray discovery number=1 Stars marked with '1', '2', or '3' have been discovered by pointed observations in the Lupus 1, Lupus 2 or Lupus 3 clouds, respectively. Left blank for stars discovered by the ROSAT All-Sky Survey. --- RAh Right Ascension for equinox 2000.0 number=2 If declination is given wit one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. h RAm Right Ascension for equinox 2000.0 number=2 If declination is given wit one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. min RAs Right Ascension for equinox 2000.0 number=2 If declination is given wit one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. s DE- Declination sign --- DEd Declination for equinox 2000.0 number=2 If declination is given wit one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. deg DEm Declination for equinox 2000.0 number=2 If declination is given wit one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. arcmin DEs Declination for equinox 2000.0 number=2 If declination is given wit one decimal only, the coordinates refer to the position of the X-ray source, otherwise the coordinates are taken from the Guide Star Catalogue. arcsec CTS ROSAT X-Ray count rate number=3 Background and vignetting corrected broadband X-ray count rate. ct/s e_CTS Error of ROSAT X-Ray count rate ct/s SpT Spectral type --- EWHa Equivalent width for H_alpha 0.1nm Vmag V magnitude number=4 Magnitudes are taken from the GSC. A value of zero means that no magnitude is available. mag Sources in pointed observations (Lupus 1) Sources in pointed observations (Lupus 2) Sources in pointed observations (Lupus 3) No Sequential number --- Star Identifier of X-ray source --- NA Note on X-ray discovery number=1 Stars marked with 'S' are also detected in the ROSAT All-Sky Survey. --- RAh Right Ascension for equinox 2000.0 number=2 Coordinates always refer to the position of the X-ray source. h RAm Right Ascension for equinox 2000.0 number=2 Coordinates always refer to the position of the X-ray source. min RAs Right Ascension for equinox 2000.0 number=2 Coordinates always refer to the position of the X-ray source. s DE- Declination sign --- DEd Declination for equinox 2000.0 number=2 Coordinates always refer to the position of the X-ray source. deg DEm Declination for equinox 2000.0 number=2 Coordinates always refer to the position of the X-ray source. arcmin DEs Declination for equinox 2000.0 number=2 Coordinates always refer to the position of the X-ray source. arcsec ML Likelihood of existence --- ExpTime Exposure time s CTS ROSAT X-Ray count rate number=3 Background and vignetting corrected broadband X-ray count rate. ct/s e_CTS Error of ROSAT X-Ray count rate ct/s HR1 ROSAT hardness ratio 1 --- e_HR1 Error of ROSAT hardness ratio 1 --- HR2 ROSAT hardness ratio 2 --- e_HR2 Error of ROSAT hardness ratio 2 --- X-ray data for new T Tauri stars in Lupus X-ray Identifier of X-ray source number=1 RXJ1507.9-4515, RXJ1533.0-3930, RXJ1539.2-4455 were found due to the SASS reduction of the RASS, but could not be detected as X-ray sources in the EXSAS reduction of the RASS. Therefore, no X-ray data are given for these stars. --- NA Note on X-ray discovery number=2 Stars marked with '1', '2', or '3' have been discovered by pointed observations in the Lupus 1, Lupus 2 or Lupus 3 clouds, respectively, and X-ray data are from pointed observations. Otherwise, X-ray data refer to the ROSAT All-Sky Survey. --- RAh Right Ascension for equinox 2000.0 number=3 Coordinates refer to the position of the X-ray source. h RAm Right Ascension for equinox 2000.0 number=3 Coordinates refer to the position of the X-ray source. min RAs Right Ascension for equinox 2000.0 number=3 Coordinates refer to the position of the X-ray source. s DE- Declination sign --- DEd Declination for equinox 2000.0 number=3 Coordinates refer to the position of the X-ray source. deg DEm Declination for equinox 2000.0 number=3 Coordinates refer to the position of the X-ray source. arcmin DEs Declination for equinox 2000.0 number=3 Coordinates refer to the position of the X-ray source. arcsec ML Likelihood of existence --- ExpTime Exposure time s CTS ROSAT X-Ray count rate number=4 Background and vignetting corrected broadband X-ray count rate. ct/s e_CTS Error of ROSAT X-Ray count rate ct/s HR1 ROSAT hardness ratio 1 --- e_HR1 Error of ROSAT hardness ratio 1 --- HR2 ROSAT hardness ratio 2 --- e_HR2 Error of ROSAT hardness ratio 2 --- Spectral fit results for new T Tauri stars in Lupus N Number --- Star Identifier of star number=1 RXJ1507.9-4515, RXJ1533.0-3930, RXJ1539.2-4455 were found due to the SASS reduction of the RASS, but could not be detected as X-ray sources in the EXSAS reduction of the RASS. Therefore, no X-ray data are given for these stars. --- NA Note on X-ray discovery number=2 Stars marked with '1', '2', or '3' have been discovered by pointed observations in the Lupus 1, Lupus 2 or Lupus 3 clouds, respectively, and X-ray data are from pointed observations. Otherwise, X-ray data refer to the ROSAT All-Sky Survey. --- AV Extinction A(V) from photometry number=3 Data from Wichmann et al., 1997A&A...320..185W mag log(HI) Absorbing HI column density number=4 Calculated from AV as given in row 4 cm-2 kTX Temperature of X-ray emitting plasma number=5 Spectral fits with hardness ratio performed with either both TX and NH as free fit parameters if no AV known, or with NH fixed and TX free if AV known. In a few cases, where AV is known, no good fit with NH fixed could be performed, hence fit was performed with both TX and NH free (in such cases both NH and NH_FIT are given). (If for TX, NH_FIT, and LX, no errors are given, no good fit could be performed, possibly because a single-temperature Raymond-Smith model is not adequate to model the star's X-ray spectrum.) keV E_kTX 1 sigma upper error bar of kTX keV e_kTX 1 sigma lower error bar of kTX keV log(NH)fit Fitted absorbing HI column density number=5 Spectral fits with hardness ratio performed with either both TX and NH as free fit parameters if no AV known, or with NH fixed and TX free if AV known. In a few cases, where AV is known, no good fit with NH fixed could be performed, hence fit was performed with both TX and NH free (in such cases both NH and NH_FIT are given). (If for TX, NH_FIT, and LX, no errors are given, no good fit could be performed, possibly because a single-temperature Raymond-Smith model is not adequate to model the star's X-ray spectrum.) cm-2 E_log(NH)fit 1 sigma upper error bar of log(NH)fit cm-2 e_log(NH)fit 1 sigma lower error bar of log(NH)fit cm-2 LX X-ray luminosity (LX/10^30^) 10-7W E_LX 1 sigma upper error bar of LX 10-7W e_LX 1 sigma lower error bar of LX 10-7W X-ray data from pointed observations and spectral fit results for T Tauri stars in Lupus known prior to our study Star Identifier of star from Schwartz (1977ApJS...35..161S) --- CTS ROSAT X-Ray count rate number=1 Background and vignetting corrected broadband X-ray count rate. Absence of error indicates that count rate is upper limit. ct/s e_CTS Error of ROSAT X-Ray count rate number=1 Background and vignetting corrected broadband X-ray count rate. Absence of error indicates that count rate is upper limit. ct/s HR1 ROSAT hardness ratio 1 --- e_HR1 Error of ROSAT hardness ratio 1 --- HR2 ROSAT hardness ratio 2 --- e_HR2 Error of ROSAT hardness ratio 2 --- AV Extinction A(V) number=2 Data from Hughes et al., 1994AJ....108.1071H mag log(NH) Absorbing HI column density number=3 Spectral fits with hardness ratio were performed with TX as free fit parameter and NH calculated from AV (Hughes et al., 1994AJ....108.1071H) In a few cases, where AV is known, no good fit with NH fixed could be performed, hence fit was performed with both TX and NH free (in such cases NH (fitted) is given). Sz 124: no good fit could be performed, possibly because a single-temperature Raymond-Smith model is not adequate to model the star's X-ray spectrum. Thus the quoted values are quite uncertain. For stars where only upper limits are known, luminosities were calculated for a Raymond-Smith spectrum with the mean temperature of kTX = 1.014 keV and NH calculated from AV. cm-2 E_log(NH) 1 sigma upper error bar of log(NH) cm-2 e_log(NH) 1 sigma lower error bar of log(NH) cm-2 kTX Temperature of X-ray emitting plasma number=3 Spectral fits with hardness ratio were performed with TX as free fit parameter and NH calculated from AV (Hughes et al., 1994AJ....108.1071H) In a few cases, where AV is known, no good fit with NH fixed could be performed, hence fit was performed with both TX and NH free (in such cases NH (fitted) is given). Sz 124: no good fit could be performed, possibly because a single-temperature Raymond-Smith model is not adequate to model the star's X-ray spectrum. Thus the quoted values are quite uncertain. For stars where only upper limits are known, luminosities were calculated for a Raymond-Smith spectrum with the mean temperature of kTX = 1.014 keV and NH calculated from AV. keV E_kTX 1 sigma upper error bar of kTX keV e_kTX 1 sigma lower error bar of kTX keV LX X-ray luminosity (LX/10^30) number=3 Spectral fits with hardness ratio were performed with TX as free fit parameter and NH calculated from AV (Hughes et al., 1994AJ....108.1071H) In a few cases, where AV is known, no good fit with NH fixed could be performed, hence fit was performed with both TX and NH free (in such cases NH (fitted) is given). Sz 124: no good fit could be performed, possibly because a single-temperature Raymond-Smith model is not adequate to model the star's X-ray spectrum. Thus the quoted values are quite uncertain. For stars where only upper limits are known, luminosities were calculated for a Raymond-Smith spectrum with the mean temperature of kTX = 1.014 keV and NH calculated from AV. 10-7W E_LX 1 sigma upper error bar of LX 10-7W e_LX 1 sigma lower error bar of LX 10-7W Patricia Bauer CDS 1996 Oct 09 Rainer Wichmann <R.Wichmann@lsw.uni-heidelberg.de> J_A+AS_123_329.xml The mean magnetic field modulus of Ap stars J/A+AS/123/353 J/A+AS/123/353 Mean magnetic field modulus of Ap stars The mean magnetic field modulus of Ap stars G Mathys S Hubrig J D Landstreet T Lanz J Manfroid Astron. Astrophys. Suppl. Ser. 123 353 1997 1997A&AS..123..353M Magnetic fields Stars, Ap stars: chemically peculiar stars: magnetic fields stars: rotation The paper reports about a systematic study of the mean magnetic field modulus of Ap stars with magnetically resolved split lines. Tables 2a and 2b present the main properties of all such stars presently known. The results about their mean magnetic field modulus derived in this study are summarized in Table 3, while the individual field measurements are given in Table 4.
Main properties of the Ap stars with resolved magnetically split lines HD HD/HDE number --- Name Other identification --- Vmag V magnitude mag SpType Spectral type --- l_Per Limit flag on rotation period number=1 >> stands for "much greater than" >~ for "greater than or approximately equal to" --- PerY Rotation period when it is expressed in years yr PerD Rotation period when it is expressed in days d u_Per Uncertainty flag on rotation period --- PerD2 Second rotation period when uncertainty on it d r_Per Code of reference for rotation period number=2 Reference codes: 1: Wolff (1975ApJ...202..127W) 2: Rice (1988A&A...199..299R) 3: Borra & Landstreet (1977ApJ...212..141B) 4: Waelkens (1985A&AS...61..127W) 5: Adelman (1981A&AS...44..265A) 6: Hensberge (1993IAUCo.138..547H) 7: Preston (1970ApJ...160.1059P) 8: Kurtz (1989MNRAS.238..261K) 9: Mathys (1991A&AS...89..121M) 10: Landstreet (unpublished; cited by Mathys 1991A&AS...89..121M) 11: Wolff (1969ApJ...158.1231W) 12: Leroy (1995A&AS..114...79L) 13: Wade et al. (1996A&A...313..209W) 14: Leroy et al. (1994A&A...284..174L) 15: Manfroid & Mathys (1996ESOSP1198....1M, A&AS, in press) 16: North & Adelman (1995A&AS..111...41N). If no reference code is given, the corresponding information comes from the present paper. --- HJD0 Phase origin (Julian Date) d Origin Property defining phase origin --- r_Origin Reference code for phase origin number=2 Reference codes: 1: Wolff (1975ApJ...202..127W) 2: Rice (1988A&A...199..299R) 3: Borra & Landstreet (1977ApJ...212..141B) 4: Waelkens (1985A&AS...61..127W) 5: Adelman (1981A&AS...44..265A) 6: Hensberge (1993IAUCo.138..547H) 7: Preston (1970ApJ...160.1059P) 8: Kurtz (1989MNRAS.238..261K) 9: Mathys (1991A&AS...89..121M) 10: Landstreet (unpublished; cited by Mathys 1991A&AS...89..121M) 11: Wolff (1969ApJ...158.1231W) 12: Leroy (1995A&AS..114...79L) 13: Wade et al. (1996A&A...313..209W) 14: Leroy et al. (1994A&A...284..174L) 15: Manfroid & Mathys (1996ESOSP1198....1M, A&AS, in press) 16: North & Adelman (1995A&AS..111...41N). If no reference code is given, the corresponding information comes from the present paper. --- Main properties of the Ap stars with resolved magnetically split lines (continued) HD/HDE HD/HDE number --- b-y Stroemgren colour index b-y mag <H>av Mean value of <H> over rotation cycle kG n_<H>av Note on <H>av number=1 A parenthesis indicates stars whose mean magnetic field modulus has not been determined throughout a complete rotation cycle yet. --- l_q Limit flag on q number=2 For stars whose mean magnetic field modulus has not been determined throughout a complete rotation cycle yet, a lower limit is given (indicated by >=, which stands for "greater than or equal to"). --- q Ratio of the maximum to the minimum of <H> --- u_q Uncertainty flag on q --- <Hz>min Observed minimum of <Hz> kG n_<Hz>min Note on <Hz>min number=3 A parenthesis indicates stars whose mean longitudinal magnetic field has not been determined throughout a complete rotation cycle yet. --- u_<Hz>min Uncertainty flag on <Hz>min --- <Hz>max Observed maximum of <Hz> kG n_<Hz>max Note on <Hz>max number=3 A parenthesis indicates stars whose mean longitudinal magnetic field has not been determined throughout a complete rotation cycle yet. --- u_<Hz>max Uncertainty flag on <Hz>max --- Discovery Date of observation of discovery of magnetically resolved lines --- r_Discovery Reference code for discovery date number=4 Reference codes: 1: Mathys (1990A&A...232..151M) 2: Mathys & Lanz (1992A&A...256..169M) 3: Mathys et al. (1993IAUCo.138..300M) 4: Preston (1971ApJ...164..309P) 5: Babel et al. (1995A&A...303L...5B) 6: Preston (1969ApJ...157..247P) 7: Preston (1970ApJ...160.1059P) 8: Preston (1969ApJ...158.1081P) 9: Didelon (1987Msngr..49....5D) 10: Adelman (1974ApJS...28...51A) 11: Scholz (1979AN....300..213S) 12: Babcock (1960ApJ...132..521B) 13: Preston & Wolff (1970ApJ...160.1071P) 14: Bonsack (1976ApJ...209..160B) 15: North (1994, in: The 25th workshop and meeting of European working group on CP stars, Jankovics I., Vincze I.J. (eds.). Gothard Astrophysical Observatory of Eotvos University, Szombathely, Hungary, p. 3) 16: Scholz & Lehmann (1988AN....309...33S) 17: Dworetsky (1982Obs...102..138D) 18: Martinez et al. (1993MNRAS.260....9M) 19: Kreidl (1985IBVS.2739....1K) 20: Neubauer (1944ApJ....99..134N) 21: Kurtz (1991MNRAS.249..468K) 22: Martinez & Kurtz (1994MNRAS.271..118M) 23: Kurtz & Martinez (1987MNRAS.226..187K) 24: Leeman (1964MNSSA..23....6L) 25: Kurtz (1983MNRAS.202....1K) If no reference code is given, the corresponding information comes from the present paper. --- Remarks See Note(5) --- r_Remarks Reference code for remarks number=4 Reference codes: 1: Mathys (1990A&A...232..151M) 2: Mathys & Lanz (1992A&A...256..169M) 3: Mathys et al. (1993IAUCo.138..300M) 4: Preston (1971ApJ...164..309P) 5: Babel et al. (1995A&A...303L...5B) 6: Preston (1969ApJ...157..247P) 7: Preston (1970ApJ...160.1059P) 8: Preston (1969ApJ...158.1081P) 9: Didelon (1987Msngr..49....5D) 10: Adelman (1974ApJS...28...51A) 11: Scholz (1979AN....300..213S) 12: Babcock (1960ApJ...132..521B) 13: Preston & Wolff (1970ApJ...160.1071P) 14: Bonsack (1976ApJ...209..160B) 15: North (1994, in: The 25th workshop and meeting of European working group on CP stars, Jankovics I., Vincze I.J. (eds.). Gothard Astrophysical Observatory of Eotvos University, Szombathely, Hungary, p. 3) 16: Scholz & Lehmann (1988AN....309...33S) 17: Dworetsky (1982Obs...102..138D) 18: Martinez et al. (1993MNRAS.260....9M) 19: Kreidl (1985IBVS.2739....1K) 20: Neubauer (1944ApJ....99..134N) 21: Kurtz (1991MNRAS.249..468K) 22: Martinez & Kurtz (1994MNRAS.271..118M) 23: Kurtz & Martinez (1987MNRAS.226..187K) 24: Leeman (1964MNSSA..23....6L) 25: Kurtz (1983MNRAS.202....1K) If no reference code is given, the corresponding information comes from the present paper. --- Summary of mean magnetic field modulus measurements HD/HDE HD/HDE number --- n_<H> Number of measurements of <H> --- Av<H> Average of all measurements of <H> G e_Av<H> Standard deviation of all <H> measurements G rms Rms deviation of <H> measurements about least-squares fit of variations by a simple function (see printed paper) G e_<H> Estimated uncertainty of <H> measurements G Mean magnetic field modulus measurements HD/HDE HD/HDE number --- HJD Heliocentric Julian Date - 2440000 d Phase Rotation phase (fraction of cycle) --- <H> Mean magnetic field modulus G Id. Code for instrumental configuration number=1 Instrumental configuration codes (see printed version for details): 1 ESO CAT + CES LC 2 ESO CAT + CES SC 3 ESO CAT + CES LC + CCD #38 4 ESO CAT + CES LC/F200 5 ESO CAT + CES SC/fibre 6 ESO 3.6 + CES LC/F200 7 OHP AURELIE 8 OHP ELODIE 9 KPNO coude feed + coude spectro 10 CFHT F/4 spectro 11 ESO NTT + EMMI --- G. Mathys ESO, Chile Patricia Bauer CDS 1997 Jan 07 Gautier Mathys <gmathys@eso.org> J_A+AS_123_353.xml On the possible variability of metallic-line and Mercury-Manganese stars J/A+AS/123/445 J/A+AS/123/445 uvby photometry of metallic & Hg-Mn stars On the possible variability of metallic-line and Mercury-Manganese stars S J Adelman Astron. Astrophys. Suppl. Ser. 123 445 1997 1997A&AS..123..445A J/A+AS/122/249 : uvby photometry of 4 CP stars (Adelman, 1997) Photometry, uvby Stars, peculiar stars: chemically peculiar stars: activity Differential Stroemgren uvby photometric observations from the 0.75-m Four College Automated Photoelectric Telescope were obtained for three metallic-line and three Mercury-Manganese stars. None were found to be variable. These sharp-lined stars may not be the best tests for class variability as their polar axes are pointed towards the earth. Each presents essentially the same visible hemisphere as it rotates.
HD 189849 15 Vul HR 7653 20 01 05.7 +27 45 13 HD 27295 53 Tau HR 1339 04 19 26.0 +21 08 34 HD 27962 68 Tau HR 1389 04 25 28.9 +17 55 43 HR 4072 HD 89822 10 24 07.9 +65 34 00 HR 6076 HD 146834 16 19 07.5 -20 13 04 omicron Peg HD 214994 HR 8641 22 41 45.3 +29 18 28
68 Tau uvby photometry 15 Vul uvby photometry omicron Peg uvby photometry 53 Tau uvby photometry HR 4072 uvby photometry HR 6076 uvby photometry HJD Heliocentric Julian Date d umag1 Variable-comparison (v-c) u magnitude mag umag2 Check-comparison (ch-c) u magnitude mag vmag1 Variable-comparison (v-c) v magnitude mag vmag2 Check-comparison (ch-c) v magnitude mag bmag1 Variable-comparison (v-c) b magnitude mag bmag2 Check-comparison (ch-c) b magnitude mag ymag1 Variable-comparison (v-c) y magnitude mag ymag2 Check-comparison (ch-c) y magnitude mag Average uvby photometry Name star name --- Per Period considered --- umag1 Variable-comparison (v-c) u magnitude mag e_umag1 rms uncertainty on umag1 mag umag2 Check-comparison (ch-c) u magnitude mag e_umag2 rms uncertainty on umag2 mag vmag1 Variable-comparison (v-c) v magnitude mag e_vmag1 rms uncertainty on vmag1 mag vmag2 Check-comparison (ch-c) v magnitude mag e_vmag2 rms uncertainty on vmag2 mag bmag1 Variable-comparison (v-c) b magnitude mag e_bmag1 rms uncertainty on bmag1 mag bmag2 Check-comparison (ch-c) b magnitude mag e_bmag2 rms uncertainty on bmag2 mag ymag1 Variable-comparison (v-c) y magnitude mag e_ymag1 rms uncertainty on ymag1 mag ymag2 Check-comparison (ch-c) y magnitude mag e_ymag2 rms uncertainty on ymag2 mag Patricia Bauer CDS 1996 Oct 15 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> UNKNOWN UNKNOWN There were an inversion between the b and v magnitude labels. This was corrected on 24-Apr-1998 J_A+AS_123_445.xml Library of high and mid-resolution spectra in the CaII H & K, H{alpha}, H{beta}, NaI D(1), D(2), and HeI D(3) line regions of F, G, K and M field stars J/A+AS/123/473 J/A+AS/123/473 Late-type star spectra Library of high and mid-resolution spectra in the CaII H & K, H{alpha}, H{beta}, NaI D(1), D(2), and HeI D(3) line regions of F, G, K and M field stars D Montes E L Martin M J Fernandez-Figueroa M Cornide E De Castro Astron. Astrophys. Suppl. Ser. 123 473 1997 1997A&AS..123..473M Spectroscopy Stars, late-type atlases stars: fundamental parameters stars: general stars: late-type In this work we present spectroscopic observations centered in the spectral lines most widely used as optical indicators of chromospheric activity (H{alpha}, H{beta}, Ca II H & K, and He I D{3}) in a sample of F, G, K and M chromospherically inactive stars. The spectra have been obtained with the aim of providing a library of high and mid-resolution spectra to be used in the application of the spectral subtraction technique to obtain the active-chromosphere contribution to these lines in chromospherically active single and binary stars. This library can also be used for spectral classification purposes. A digital version with all the spectra is available via ftp and the World Wide Web (WWW) in both ASCII and FITS formats
List of stars, Spectral type and name of the corresponding FITS spectra RAh Right Ascension J2000 (hours) number=1 Position from SIMBAD (added in September 1998); the Sun is the only star without its position. h RAm Right Ascension J2000 (minutes) number=1 Position from SIMBAD (added in September 1998); the Sun is the only star without its position. min RAs Right Ascension J2000 (seconds) number=1 Position from SIMBAD (added in September 1998); the Sun is the only star without its position. s DE- Declination J2000 (sign) number=1 Position from SIMBAD (added in September 1998); the Sun is the only star without its position. --- DEd Declination J2000 (degrees) number=1 Position from SIMBAD (added in September 1998); the Sun is the only star without its position. deg DEm Declination J2000 (minutes) number=1 Position from SIMBAD (added in September 1998); the Sun is the only star without its position. arcmin DEs Declination J2000 (seconds) number=1 Position from SIMBAD (added in September 1998); the Sun is the only star without its position. arcsec Instr Instrument and wavelength range number=2 The codes are 1 = Feb 1988, tel.: 2.2m, CaII H&K: wavelength range: 3890-4009, res.: 0.198 2 = Jul 1989, tel.: 2.2m, H{alpha}: wavelength range: 6464-6719, res.: 0.50 3 = Jul 1989, tel.: 2.2m, CaII H&K: wavelength range: 3883-4015, res.: 0.198 4 = Dec 1992, tel.: INT, H{beta}: wavelength range: 4778-4941, res.: 0.34 5 = Dec 1992, tel.: INT, H{alpha}: wavelength range: 6507-6764, res.: 0.45 6 = Dec 1992, tel.: INT, CaII H&K: wavelength range: 3840-4050, res.: 0.358 7 = Mar 1993, tel.: 2.2m, CaII H&K: wavelength range: 3830-4018, res.: 0.420 8 = Jun 1995, tel.: 2.2m, H{beta}: wavelength range: 4807-4926, res.: 0.26 9 = Jun 1995, tel.: 2.2m, H{alpha}: wavelength range: 6510-6638, res.: 0.26 10 = Sep 1995, tel.: INT, H{alpha}: wavelength range: 6452-6695, res.: 0.48 11 = Sep 1995, tel.: INT, He I: wavelength range: 5762-6011, res.: 0.48 12 = Jan 1993, tel.: WHT, H{alpha}: wavelength range: 5500-7000, res.: 2.90 13 = Apr 1993, tel.: INT, H{alpha}: wavelength range: 5626-7643, res.: 3.16 14 = Jun 1995, tel.: INT, H{alpha}: wavelength range: 6430-6824, res.: 0.78 15 = Aug 1995, tel.: INT, H{alpha}: wavelength range: 6295-6918, res.: 1.06 16 = Nov 1995, tel.: INT, H{alpha}: wavelength range: 6344-6742, res.: 0.78 --- HD HD number --- HR HR number --- Name name of the star --- Sp Spectral type --- FITSfile Name of FITS file, in subdirectory sp number=3 File were renamed in Spectember 1998 (limit of 8+3 characters); the filename includes the Instr number. --- Spectrum Orignal file name number=3 File were renamed in Spectember 1998 (limit of 8+3 characters); the filename includes the Instr number. --- Patricia Bauer, Francois Ochsenbein CDS 1998 Sep 10 David Monte <dmg@astro4.fis.ucm.es> UNKNOWN UNKNOWN * 02-Oct-1996: Archived as received * 10-Sep-1998: positions added in the list of stars J_A+AS_123_473.xml CCD measurements of double and multiple stars in Belgrade J/A+AS/123/487 J/A+AS/123/487 CCD measurements of double and multiple stars CCD measurements of double and multiple stars in Belgrade G M Popovic R Pavlovic Astron. Astrophys. Suppl. Ser. 123 487 1997 1997A&AS..123..487P Positional data Stars, double and multiple astrometry binaries: visual The CCD measurements for 123 double stars with ST-6 camera attached to the Zeiss 65/1055 cm Refractor of the Belgrade Observatory are communicated.
CCD measurements WDS WDS designation (Catalogue <I/107>) --- Name Designation of the pair discoverer --- Mult Multiplicity --- Date Observation date yr PA Position angle deg rho Angular separation of the components arcsec Auth Author performing the measurement --- o_Auth Number of measurements --- Obs Designation of the authors having obtained the image number=1 POP = Popovic, PAV = Pavlovic, TRA = Trajkovska --- ADS Number in ADS catalogue --- Notes * indicates a note in table2 --- Notes ADS ADS name --- Name Other name --- Com Comments --- table1.tex TeX version of table1 Patricia Bauer CDS 1996 Oct 07 Rade Pavlovic <prade@EUnet.yu> J_A+AS_123_487.xml A photometric study of the Bright Cloud B in Sagittarius. VIII. 1061 new variable stars. J/A+AS/123/507 J/A+AS/123/507 New variables in Sagittarius A photometric study of the Bright Cloud B in Sagittarius. VIII. 1061 new variable stars. A Terzan A Bernard J Guibert Astron. Astrophys. Suppl. Ser. 123 507 1997 1997A&AS..123..507T J/A+AS/49/715 : (621 variables) J/A+AS/76/205 : (1592 variables and 30 diffuse objects), Paper VI J/A+AS/90/451 : (1165 variables and 65 diffuse objects), Paper VII 1077Msngr..10....1T, Terzan, Paper I 1978Msngr..15...14T, Terzan and Bernard, Paper II 1980Msngr..20....6T, Terzan and Ju, Paper III 1985Msngr..42....4T, Terzan, Paper IV 1987A&AS...67..309T, Terzan et al., Paper V 1988A&AS...76..205T, Terzan and Ounnas, Paper VI 1991A&AS...90..451T, Terzan and Gosset, Paper VII Magnitudes Stars, variable Galaxy: center Galaxy: structure stars: AGB and post-AGB stars: variables: general For the coordinates and identification charts of the variables discovered in the other parts of the surveyed region, see references in the publication. A compilation of all the (~4000) variables discovered in the entire 100 square-degree surveyed region in the course of this programme, is in preparation and will be available at CDS in electronic form.
*New variable stars discovered in Field C Ter Terzan number (blank for the 13 variables from GCVS) --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec GLON Galactic longitude lII deg GLAT Galactic latitude bII deg l_Rmax Limit flag on Rmax --- Rmax R Magnitude at maximum mag n_Rmax Plate code for maximum number=1 For plate codes, see Table 2 in the publication --- Rmin R Magnitude at minimum mag n_Rmin Plate code for minimum number=1 For plate codes, see Table 2 in the publication --- RAmpl Observed R amplitude mag n_RAmpl Notes about magnitudes number=2 Magnitudes at minimum or maximum: *: Rmin is a lower limit +: Rmin is an upper limit #: Rmax is an upper limit --- GCVS Name of GCVS objects --- Patricia Bauer CDS 1996 Nov 12 Jean Guibert <guibert@sm10a.obspm.fr> J_A+AS_123_507.xml Surveys of ultraviolet-excess quasar candidates in large fields. The area around NGC 450 J/A+AS/123/529 J/A+AS/123/529 UV-excess quasar candidates around NGC 450 Surveys of ultraviolet-excess quasar candidates in large fields. The area around NGC 450 E Gosset O Moreau J Surdej Astron. Astrophys. Suppl. Ser. 123 529 1997 1997A&AS..123..529G Photometry, UBV QSOs Redshifts quasars: general surveys We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.
Catalogue of quasars and quasar candidates RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s u_RAs ":" slightly less precise value --- DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec u_DEs ":" slightly less precise value --- z Redshift --- u_z ":" uncertain value "?" very uncertain value --- Name Object name number=1 B1950 name of the quasar, or an indication of the nature of the object (if it is not a quasar, e.G. STAR), or simply states that the object is still an unidentified candidate (C). --- P/S Primary (P) or secondary (S) candidate --- n_P/S * when the spectrum of the object is available in fig.2 of the paper. --- --- --- NGC450 Internal identification number in the present survey (NGC450 # "NGC450") --- n_NGC450 Flag indicating a note in notes.dat file --- --- --- NGC520 Identification number in the NGC 520 survey (NGC520 # 'NGC520') --- m_NGC520 Multiplicity index on NGC520 --- l_Bmag Limit flag on Bmag --- Bmag B magnitude mag u_Bmag Uncertainty flag on Bmag --- l_Umag Limit flag on Umag --- Umag U magnitude mag u_Umag Uncertainty flag on Umag --- l_U-B Limit flag on U-B --- U-B U-B colour index mag u_U-B Uncertainty flag on U-B --- Spect Spectroscopy number=2 Identification of the spectroscopic runs with the exposure time in seconds. --- Individual notes NGC450 NGC450 internal designation --- Note Text of the note --- Patricia Bauer CDS 1997 Dec 02 Eric Gosset <gosset@astro.ulg.ac.be> J_A+AS_123_529.xml Atomic data from the Iron Project. XXIII. Relativistic rate coefficients for Fe XXII with inclusion of radiation damping. J/A+AS/123/575 J/A+AS/123/575 IRON Project XXIII. Fe XXII excitation rate Atomic data from the Iron Project. XXIII. Relativistic rate coefficients for Fe XXII with inclusion of radiation damping. H L Zhang A K Pradhan Astron. Astrophys. Suppl. Ser. 123 575 1997 1997A&AS..123..575Z J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions J/A+AS/123/159 : IRON Project XXII. C and O radiative rates 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths 1997A&AS..122..167B : IRON Project XX. Fe I oscillator strengths 1997A&AS..122..177P : IRON Project XXI. Fe I fine-structure transition Atomic physics atomic data Sun: flares X-rays: general New collision strengths have been calculated for 990 transitions among 45 fine structure n=2 and n=3 levels of Fe XXII. The relativistic Breit-Pauli formulation of the R-matrix method was employed in the close coupling approximation, with radiation damping of autoionizing resonances included for the first time in the calculations of excitation rate coefficients. It is found that, at low temperatures, the relativistic effects considerably enhance rate coefficients for the intercombination transitions, and the radiation damping effect reduces those for a few transitions. It is also found that resonances due to coupling with the n=3 levels significantly enhance rate coefficients for the transitions to low-lying levels at intermediate and high temperatures, and for the transitions to the n=2 high-lying levels at all temperatures. It is expected that the new data, tabulated at a wide range of temperatures, would lead to a revision of the spectral diagnostics of Fe XXII in laboratory and astrophysical sources, in particular the X-ray spectra observed from solar flares and tokamaks.
Levels for table3 Levels for table4 Levels for table5 Index Level index --- Conf Electronic configuration --- Term Electronic term --- J Total angular momentum --- E Theoretical energy Ry Patricia Bauer CDS 1996 Nov 12 Honglin Zhang <zhang@payne.mps.ohio-state.edu> J_A+AS_123_575.xml Four colour photometry of late-type binary systems. II. New light curves of BH Virginis J/A+AS/123/59 J/A+AS/123/59 uvby photometry of BH Vir Four colour photometry of late-type binary systems. II. New light curves of BH Virginis R Clement M Garcia V Reglero J V Clausen A Bravo J Suso J Fabregat Astron. Astrophys. Suppl. Ser. 123 59 1997 1997A&AS..123...59C J/A+AS/123/1 : uvbyBeta photometry of ZZ UMa (Clement+ 1997) Binaries, eclipsing Photometry binaries: eclipsing stars: individual (BH Vir) This paper presents new complete uvby light curves of the late-type detached eclipsing binary BH Vir (G0V + G5V, P=0.81687099d). This binary system has been observed during four campaigns at the Calar Alto Observatory (Almeria, Spain) and at the European Southern Observatory (La Silla, Chile). This observations are part of a 6 year uvby and H{beta} monitoring program of low mass eclipsing binaries which main objective is to provide accurate absolute astrophysical parameters for late-type main sequence stars. 1585 points spreaded over the binary period and covering both eclipses are given. The internal accuracy of the standard photometry measured as the mean RMS of the differences between standard value and observed value for the standard stars observed along the program is quoted in a few millimagnitudes. Detailed analysis of BH Vir, based on these light curves, will be published separately.
Differential magnitudes (BH Vir - HD 121935) HJD Heliocentric Julian day d Dumag Differential u magnitude mag Dvmag Differential v magnitude mag Dbmag Differential b magnitude mag Dymag Differential y magnitude mag table2a.tex LaTeX version of table2 (part 1) table2b.tex LaTeX version of table2 (part 2) Patricia Bauer CDS 1996 Sep 28 Rosa Clement <clement@deneb.matapl.uv.es> J_A+AS_123_59.xml A multiwavelength study of star formation in the very young open cluster NGC 6530 J/A+AS/123/63 J/A+AS/123/63 NGC 6530 multiwavelength photometry A multiwavelength study of star formation in the very young open cluster NGC 6530 M E van den Ancker P S The A Feinstein R A Vazquez D de Winter M R Perez Astron. Astrophys. Suppl. Ser. 123 63 1997 1997A&AS..123...63V Clusters, open Photometry circumstellar matter dust, extinction HII regions open clusters and associations: individual (NGC 6530) stars: formation stars: pre-main sequence The distance and formation history of the very young open cluster NGC 6530 were investigated by studying a total of 132 probable member stars of this open cluster. It was concluded that the distance to NGC 6530 is 1.8+/-0.2kpc, and its interstellar reddening E(B-V) is 0.30. Furthermore, we conclude that the extinction law of the intracluster material is normal (i.e. R_V=3.1), but anomalous extinction laws were found for several more embedded stars in the cluster. Of the 132 stars included in this study, 11 are suspected to be variable, five show Halpha in emission and nine show an infrared excess. Among the member stars of NGC 6530, three were found to be part of the Herbig Ae/Be stellar class, whereas two others are possible members of this stellar group as well. Also, one cluster member is probably a new massive post-AGB star, whereas the same could possibly apply to another member star. Finally, from the distribution of post- and pre-main sequence stars in the cluster's HR-diagram, it was concluded that the process of star formation in NGC 6530 must have started a few times 10^7 years ago and, for the less massive stars, is probably still going on today.
Properties of programme stars in NGC 6530 from literature VAJ Star number by van Altena & Jones (1972A&A....20..425V) --- Walk Star number by Walker (1957ApJ...125..636W) and Kilambi (1977MNRAS.178..423K) --- Sag Star number by Sagar & Joshi (1978MNRAS.184..467S) --- Other Other designation --- RAh Right ascension (J1950) h RAm Right ascension (J1950) min RAs Right ascension (J1950) s DE- Declination sign --- DEd Declination (J1950) deg DEm Declination (J1950) arcmin DEs Declination (J1950) arcsec Prob Proper motion membership probability % Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag HRV Heliocentric radial velocity km/s Sp Spectral type --- Ref. Reference for spectral type number=1 1: Buscombe 1984, See Cat. <III/189> 2: Boggs & Boehm-Vitense (1989ApJ...339..209B) 3: Walker (1957ApJ...125..636W) 4: Johnson & Borgman (1963BAN....17..115J) 5: Hiltner et al. (1965ApJ...141..183H) 6: Torres (1987ApJ...322..949T) 7: Boesono et al. (1987Ap&SS.137..167B) 8: Morrison & Conti (1978ApJ...224..558M) --- New photometric data of stars in NGC 6530 No. Star number for new stars --- Vmag Walraven V intensity --- Vmag1 Johnson V magnitude computed from Walraven V and V-B mag V-B Walraven V-B colour index --- B-U Walraven B-U colour index --- U-W Walraven U-W colour index --- B-L Walraven D-L colour index --- Date1 Date (dd/mm/yy) of Walraven measurement --- Vmag2 Johnson V magnitude mag B-V Johnson B-V colour index mag U-B Johnson U-B colour index mag V-R Cousins V-R colour index mag V-I Cousins V-I colour index mag Date2 Date (dd/mm/yy) of UBVRI measurement --- Jmag ESO J magnitude index mag Hmag ESO H magnitude index mag Kmag ESO K magnitude index mag Date3 Date (dd/mm/yy) of JHK measurement --- Remark Remarks number=1 1: Probably a variable star. 2: Two sources at that position in the infrared. --- Astrophysical parameters of stars in NGC 6530 No Star number --- SpUBVl Spectral type from UBV data from literature --- SpUBVn Spectral type from new UBV data --- SpWalr Spectral type from new Walraven data --- SpIDS Spectral type from IDS spectrum --- SpCCD Spectral type from CCD spectrum --- SpAdop Adopted spectral type --- E(B-V) B-V colour excess mag Extinct Ratio of visual to selective extinction --- u_Extinct Uncertainty flag on extinct --- Dist Photometric distance kpc logTeff log of effective temperature K logL log of stellar luminosity solLum IRexcess Presence of infrared excess (YES/NO) --- Patricia Bauer CDS 1996 Sep 13 Mario van den Ancker <MARIO@astro.uva.nl> J_A+AS_123_63.xml A consolidated catalogue of lambda Bootis stars J/A+AS/123/93 J/A+AS/123/93 Lambda Boo stars consolidated catalogue A consolidated catalogue of lambda Bootis stars E Paunzen W W Weiss U Heiter P North Astron. Astrophys. Suppl. Ser. 123 93 1997 1997A&AS..123...93P Magnitudes Rotational velocities Stars, peculiar astronomical data bases: miscellaneous catalogs stars: chemically peculiar stars: early-type stars: individual (Lambda Boo) This paper describes the first steps towards the homogenization of the lambda Bootis group, leading to a concise definition of lambda Bootis stars: Population I, hydrogen burning, metal poor (except of C, N, O and S) A to F-type stars. The definition does not depend on phenomenological features, like flux depressions, colour excesses, vsini values, etc. Based on this new homogeneous catalogue with 45 lambda Bootis stars, we discuss classification criteria which can be used for a spectroscopic and photometric all-sky survey for lambda Bootis stars in the field and in clusters of different ages.
Catalogue of lambda Bootis stars HD HD number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec vsini Rotational velocity km/s r_vsini Reference on rotational velocity number=1 A: Gray R.O., Corbally C.J., 1993AJ....106..632G B: Uesugi A., Fukuda I., 1982, Revised Catalogue of Stellar Rotational Velocities, Department of Astronomy, Kyoto Univ., Kyoto C: North P., Berthet S., Lanz T., 1994A&A...281..775N D: Stuerenburg S., 1993A&A...277..139S E: Abt H.A., Morrell N.I., 1995ApJS...99..135A F: Holweger H., Rentzsch-Holm I., 1995A&A...303..819H --- Vmag V magnitude mag Note * indicates combined magnitude for binary --- CS Reference on classification spectroscopy number=2 References: AB79 : Abt H.A., Brodzik D., Schaefer B., 1979PASP...91..176A AB84a: Abt H.A., 1984ApJ...285..247A AB84b: Abt H.A., 1984, In: Garrison R.F. (ed.) The MK Process and Stellar Classification. David Dunlap Observatory, Toronto, p. 340 AB85 : Abt H.A., 1985ApJS...59...95A ADS : Binary catalogue entry AN77 : Andersen J., Nordstroem B., 1977A&AS...29..309A AT78 : Antonello E., Arienti F., Frascassini M., Passinetti L.E., 1978A&A....66..374A BA69 : Baschek B., Searle L., 1969ApJ...155..537B BA84 : Baschek B., Heck A., Jaschek C., et al., 1984A&A...131...37B BL77 : Balona L.A., 1977MNRAS..84..101B BA88 : Baschek B., Slettebak A., 1988A&A...207..112B BO90 : Bohlender D.A., Landstreet J.D., 1990MNRAS.247..606B BO94 : Bohlender D.A., Walker G.A.H., 1994MNRAS.266..891B BR79 : Breger M., 1979PASP...91....5B FA90 : Faraggiana R., Gerbaldi M., Boehm C., 1990A&A...235..311F GI77 : Gies D.R., Percy J.R., 1977AJ.....82..166G GR88 : Gray R.O., 1988AJ.....95..220G GR93 : Gray R.O., Corbally C.J., 1993AJ....106..632G HA83 : Hauck B., Slettebak A., 1983A&A...127..231H HA86 : Hauck B., 1986A&A...154..349H HE96 : Heiter U., 1996, Master Thesis, University Vienna HO91 : Holweger H, Stuerenburg S., 1991A&A...252..255H IDS : Binary catalogue entry (see WDS, Cat. <I/237>) IL95 : Iliev I.K., Barzova I.S., 1995A&A...302..735I KU94a: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4069....1K KU94b: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4070....1K KU96a: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4310....1K KU96b: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4349....1K KS96 : Kusakin A.V., Mkrtichian D.E., 1996IBVS.4314....1K LE94 : Levato H., Malaroda S., Grosso M., Morrell N.I., 1994, PASPC 60, 93 NVS : suspected variable star OK67 : Oke J.B., 1967ApJ...150..513O PA94a: Paunzen E., Weiss W.W., 1994IBVS.3986....1P PA94b: Paunzen E., Handler G., Weiss W.W., North P., 1994IBVS.4094....1P PA95a: Paunzen E., Heiter U., Weiss W.W., 1995IBVS.4191....1P PA95b: Paunzen E., 1995IBVS.4254....1P PA95c: Paunzen E., Duffee B., 1995IBVS.4255....1P PA96a: Paunzen E., Handler G., 1996IBVS.4301....1P PA96b: Paunzen E., Weiss W.W., Kuschnig R., 1996IBVS.4302....1P (+erratum in 1996IBVS.4349....1K) PA96c: Paunzen E., Handler G., 1996IBVS.4318....1P PA96d: Paunzen E., Handler G., Weiss W.W., 1996IBVS.4351....1P RU82 : Rufener F., Bartholdi P., 1982A&AS...48..503R SL52 : Slettebak A., 1952ApJ...115..575S SL54 : Slettebak A., 1954ApJ...119..146S SL68 : Slettebak A., Wright R.R., Graham J.A., 1968AJ.....73..152S ST93 : Stuerenburg S., 1993A&A...277..139S VE90 : Venn K.A., Lambert D.L., 1990ApJ...363..234V WA83 : Waelkens C., Rufener F., 1983BHarO...7..301W WE94 : Weiss W.W., Paunzen E., Kuschnig R., Schneider H., 1994A&A...281..797W --- HS Reference on high resolution spectroscopy number=2 References: AB79 : Abt H.A., Brodzik D., Schaefer B., 1979PASP...91..176A AB84a: Abt H.A., 1984ApJ...285..247A AB84b: Abt H.A., 1984, In: Garrison R.F. (ed.) The MK Process and Stellar Classification. David Dunlap Observatory, Toronto, p. 340 AB85 : Abt H.A., 1985ApJS...59...95A ADS : Binary catalogue entry AN77 : Andersen J., Nordstroem B., 1977A&AS...29..309A AT78 : Antonello E., Arienti F., Frascassini M., Passinetti L.E., 1978A&A....66..374A BA69 : Baschek B., Searle L., 1969ApJ...155..537B BA84 : Baschek B., Heck A., Jaschek C., et al., 1984A&A...131...37B BL77 : Balona L.A., 1977MNRAS..84..101B BA88 : Baschek B., Slettebak A., 1988A&A...207..112B BO90 : Bohlender D.A., Landstreet J.D., 1990MNRAS.247..606B BO94 : Bohlender D.A., Walker G.A.H., 1994MNRAS.266..891B BR79 : Breger M., 1979PASP...91....5B FA90 : Faraggiana R., Gerbaldi M., Boehm C., 1990A&A...235..311F GI77 : Gies D.R., Percy J.R., 1977AJ.....82..166G GR88 : Gray R.O., 1988AJ.....95..220G GR93 : Gray R.O., Corbally C.J., 1993AJ....106..632G HA83 : Hauck B., Slettebak A., 1983A&A...127..231H HA86 : Hauck B., 1986A&A...154..349H HE96 : Heiter U., 1996, Master Thesis, University Vienna HO91 : Holweger H, Stuerenburg S., 1991A&A...252..255H IDS : Binary catalogue entry (see WDS, Cat. <I/237>) IL95 : Iliev I.K., Barzova I.S., 1995A&A...302..735I KU94a: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4069....1K KU94b: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4070....1K KU96a: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4310....1K KU96b: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4349....1K KS96 : Kusakin A.V., Mkrtichian D.E., 1996IBVS.4314....1K LE94 : Levato H., Malaroda S., Grosso M., Morrell N.I., 1994, PASPC 60, 93 NVS : suspected variable star OK67 : Oke J.B., 1967ApJ...150..513O PA94a: Paunzen E., Weiss W.W., 1994IBVS.3986....1P PA94b: Paunzen E., Handler G., Weiss W.W., North P., 1994IBVS.4094....1P PA95a: Paunzen E., Heiter U., Weiss W.W., 1995IBVS.4191....1P PA95b: Paunzen E., 1995IBVS.4254....1P PA95c: Paunzen E., Duffee B., 1995IBVS.4255....1P PA96a: Paunzen E., Handler G., 1996IBVS.4301....1P PA96b: Paunzen E., Weiss W.W., Kuschnig R., 1996IBVS.4302....1P (+erratum in 1996IBVS.4349....1K) PA96c: Paunzen E., Handler G., 1996IBVS.4318....1P PA96d: Paunzen E., Handler G., Weiss W.W., 1996IBVS.4351....1P RU82 : Rufener F., Bartholdi P., 1982A&AS...48..503R SL52 : Slettebak A., 1952ApJ...115..575S SL54 : Slettebak A., 1954ApJ...119..146S SL68 : Slettebak A., Wright R.R., Graham J.A., 1968AJ.....73..152S ST93 : Stuerenburg S., 1993A&A...277..139S VE90 : Venn K.A., Lambert D.L., 1990ApJ...363..234V WA83 : Waelkens C., Rufener F., 1983BHarO...7..301W WE94 : Weiss W.W., Paunzen E., Kuschnig R., Schneider H., 1994A&A...281..797W --- UV Reference on UV observations number=2 References: AB79 : Abt H.A., Brodzik D., Schaefer B., 1979PASP...91..176A AB84a: Abt H.A., 1984ApJ...285..247A AB84b: Abt H.A., 1984, In: Garrison R.F. (ed.) The MK Process and Stellar Classification. David Dunlap Observatory, Toronto, p. 340 AB85 : Abt H.A., 1985ApJS...59...95A ADS : Binary catalogue entry AN77 : Andersen J., Nordstroem B., 1977A&AS...29..309A AT78 : Antonello E., Arienti F., Frascassini M., Passinetti L.E., 1978A&A....66..374A BA69 : Baschek B., Searle L., 1969ApJ...155..537B BA84 : Baschek B., Heck A., Jaschek C., et al., 1984A&A...131...37B BL77 : Balona L.A., 1977MNRAS..84..101B BA88 : Baschek B., Slettebak A., 1988A&A...207..112B BO90 : Bohlender D.A., Landstreet J.D., 1990MNRAS.247..606B BO94 : Bohlender D.A., Walker G.A.H., 1994MNRAS.266..891B BR79 : Breger M., 1979PASP...91....5B FA90 : Faraggiana R., Gerbaldi M., Boehm C., 1990A&A...235..311F GI77 : Gies D.R., Percy J.R., 1977AJ.....82..166G GR88 : Gray R.O., 1988AJ.....95..220G GR93 : Gray R.O., Corbally C.J., 1993AJ....106..632G HA83 : Hauck B., Slettebak A., 1983A&A...127..231H HA86 : Hauck B., 1986A&A...154..349H HE96 : Heiter U., 1996, Master Thesis, University Vienna HO91 : Holweger H, Stuerenburg S., 1991A&A...252..255H IDS : Binary catalogue entry (see WDS, Cat. <I/237>) IL95 : Iliev I.K., Barzova I.S., 1995A&A...302..735I KU94a: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4069....1K KU94b: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4070....1K KU96a: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4310....1K KU96b: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4349....1K KS96 : Kusakin A.V., Mkrtichian D.E., 1996IBVS.4314....1K LE94 : Levato H., Malaroda S., Grosso M., Morrell N.I., 1994, PASPC 60, 93 NVS : suspected variable star OK67 : Oke J.B., 1967ApJ...150..513O PA94a: Paunzen E., Weiss W.W., 1994IBVS.3986....1P PA94b: Paunzen E., Handler G., Weiss W.W., North P., 1994IBVS.4094....1P PA95a: Paunzen E., Heiter U., Weiss W.W., 1995IBVS.4191....1P PA95b: Paunzen E., 1995IBVS.4254....1P PA95c: Paunzen E., Duffee B., 1995IBVS.4255....1P PA96a: Paunzen E., Handler G., 1996IBVS.4301....1P PA96b: Paunzen E., Weiss W.W., Kuschnig R., 1996IBVS.4302....1P (+erratum in 1996IBVS.4349....1K) PA96c: Paunzen E., Handler G., 1996IBVS.4318....1P PA96d: Paunzen E., Handler G., Weiss W.W., 1996IBVS.4351....1P RU82 : Rufener F., Bartholdi P., 1982A&AS...48..503R SL52 : Slettebak A., 1952ApJ...115..575S SL54 : Slettebak A., 1954ApJ...119..146S SL68 : Slettebak A., Wright R.R., Graham J.A., 1968AJ.....73..152S ST93 : Stuerenburg S., 1993A&A...277..139S VE90 : Venn K.A., Lambert D.L., 1990ApJ...363..234V WA83 : Waelkens C., Rufener F., 1983BHarO...7..301W WE94 : Weiss W.W., Paunzen E., Kuschnig R., Schneider H., 1994A&A...281..797W --- VAR Reference on photometric survey number=2 References: AB79 : Abt H.A., Brodzik D., Schaefer B., 1979PASP...91..176A AB84a: Abt H.A., 1984ApJ...285..247A AB84b: Abt H.A., 1984, In: Garrison R.F. (ed.) The MK Process and Stellar Classification. David Dunlap Observatory, Toronto, p. 340 AB85 : Abt H.A., 1985ApJS...59...95A ADS : Binary catalogue entry AN77 : Andersen J., Nordstroem B., 1977A&AS...29..309A AT78 : Antonello E., Arienti F., Frascassini M., Passinetti L.E., 1978A&A....66..374A BA69 : Baschek B., Searle L., 1969ApJ...155..537B BA84 : Baschek B., Heck A., Jaschek C., et al., 1984A&A...131...37B BL77 : Balona L.A., 1977MNRAS..84..101B BA88 : Baschek B., Slettebak A., 1988A&A...207..112B BO90 : Bohlender D.A., Landstreet J.D., 1990MNRAS.247..606B BO94 : Bohlender D.A., Walker G.A.H., 1994MNRAS.266..891B BR79 : Breger M., 1979PASP...91....5B FA90 : Faraggiana R., Gerbaldi M., Boehm C., 1990A&A...235..311F GI77 : Gies D.R., Percy J.R., 1977AJ.....82..166G GR88 : Gray R.O., 1988AJ.....95..220G GR93 : Gray R.O., Corbally C.J., 1993AJ....106..632G HA83 : Hauck B., Slettebak A., 1983A&A...127..231H HA86 : Hauck B., 1986A&A...154..349H HE96 : Heiter U., 1996, Master Thesis, University Vienna HO91 : Holweger H, Stuerenburg S., 1991A&A...252..255H IDS : Binary catalogue entry (see WDS, Cat. <I/237>) IL95 : Iliev I.K., Barzova I.S., 1995A&A...302..735I KU94a: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4069....1K KU94b: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4070....1K KU96a: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4310....1K KU96b: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4349....1K KS96 : Kusakin A.V., Mkrtichian D.E., 1996IBVS.4314....1K LE94 : Levato H., Malaroda S., Grosso M., Morrell N.I., 1994, PASPC 60, 93 NVS : suspected variable star OK67 : Oke J.B., 1967ApJ...150..513O PA94a: Paunzen E., Weiss W.W., 1994IBVS.3986....1P PA94b: Paunzen E., Handler G., Weiss W.W., North P., 1994IBVS.4094....1P PA95a: Paunzen E., Heiter U., Weiss W.W., 1995IBVS.4191....1P PA95b: Paunzen E., 1995IBVS.4254....1P PA95c: Paunzen E., Duffee B., 1995IBVS.4255....1P PA96a: Paunzen E., Handler G., 1996IBVS.4301....1P PA96b: Paunzen E., Weiss W.W., Kuschnig R., 1996IBVS.4302....1P (+erratum in 1996IBVS.4349....1K) PA96c: Paunzen E., Handler G., 1996IBVS.4318....1P PA96d: Paunzen E., Handler G., Weiss W.W., 1996IBVS.4351....1P RU82 : Rufener F., Bartholdi P., 1982A&AS...48..503R SL52 : Slettebak A., 1952ApJ...115..575S SL54 : Slettebak A., 1954ApJ...119..146S SL68 : Slettebak A., Wright R.R., Graham J.A., 1968AJ.....73..152S ST93 : Stuerenburg S., 1993A&A...277..139S VE90 : Venn K.A., Lambert D.L., 1990ApJ...363..234V WA83 : Waelkens C., Rufener F., 1983BHarO...7..301W WE94 : Weiss W.W., Paunzen E., Kuschnig R., Schneider H., 1994A&A...281..797W --- IR IR observations available --- Geneva Geneva colours available --- Stroemgren Stroemgren colours available --- Ref Additional references number=2 References: AB79 : Abt H.A., Brodzik D., Schaefer B., 1979PASP...91..176A AB84a: Abt H.A., 1984ApJ...285..247A AB84b: Abt H.A., 1984, In: Garrison R.F. (ed.) The MK Process and Stellar Classification. David Dunlap Observatory, Toronto, p. 340 AB85 : Abt H.A., 1985ApJS...59...95A ADS : Binary catalogue entry AN77 : Andersen J., Nordstroem B., 1977A&AS...29..309A AT78 : Antonello E., Arienti F., Frascassini M., Passinetti L.E., 1978A&A....66..374A BA69 : Baschek B., Searle L., 1969ApJ...155..537B BA84 : Baschek B., Heck A., Jaschek C., et al., 1984A&A...131...37B BL77 : Balona L.A., 1977MNRAS..84..101B BA88 : Baschek B., Slettebak A., 1988A&A...207..112B BO90 : Bohlender D.A., Landstreet J.D., 1990MNRAS.247..606B BO94 : Bohlender D.A., Walker G.A.H., 1994MNRAS.266..891B BR79 : Breger M., 1979PASP...91....5B FA90 : Faraggiana R., Gerbaldi M., Boehm C., 1990A&A...235..311F GI77 : Gies D.R., Percy J.R., 1977AJ.....82..166G GR88 : Gray R.O., 1988AJ.....95..220G GR93 : Gray R.O., Corbally C.J., 1993AJ....106..632G HA83 : Hauck B., Slettebak A., 1983A&A...127..231H HA86 : Hauck B., 1986A&A...154..349H HE96 : Heiter U., 1996, Master Thesis, University Vienna HO91 : Holweger H, Stuerenburg S., 1991A&A...252..255H IDS : Binary catalogue entry (see WDS, Cat. <I/237>) IL95 : Iliev I.K., Barzova I.S., 1995A&A...302..735I KU94a: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4069....1K KU94b: Kuschnig R., Paunzen E., Weiss W.W., 1994IBVS.4070....1K KU96a: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4310....1K KU96b: Kuschnig R., Gelbmann M., Paunzen E., Weiss W.W., 1996IBVS.4349....1K KS96 : Kusakin A.V., Mkrtichian D.E., 1996IBVS.4314....1K LE94 : Levato H., Malaroda S., Grosso M., Morrell N.I., 1994, PASPC 60, 93 NVS : suspected variable star OK67 : Oke J.B., 1967ApJ...150..513O PA94a: Paunzen E., Weiss W.W., 1994IBVS.3986....1P PA94b: Paunzen E., Handler G., Weiss W.W., North P., 1994IBVS.4094....1P PA95a: Paunzen E., Heiter U., Weiss W.W., 1995IBVS.4191....1P PA95b: Paunzen E., 1995IBVS.4254....1P PA95c: Paunzen E., Duffee B., 1995IBVS.4255....1P PA96a: Paunzen E., Handler G., 1996IBVS.4301....1P PA96b: Paunzen E., Weiss W.W., Kuschnig R., 1996IBVS.4302....1P (+erratum in 1996IBVS.4349....1K) PA96c: Paunzen E., Handler G., 1996IBVS.4318....1P PA96d: Paunzen E., Handler G., Weiss W.W., 1996IBVS.4351....1P RU82 : Rufener F., Bartholdi P., 1982A&AS...48..503R SL52 : Slettebak A., 1952ApJ...115..575S SL54 : Slettebak A., 1954ApJ...119..146S SL68 : Slettebak A., Wright R.R., Graham J.A., 1968AJ.....73..152S ST93 : Stuerenburg S., 1993A&A...277..139S VE90 : Venn K.A., Lambert D.L., 1990ApJ...363..234V WA83 : Waelkens C., Rufener F., 1983BHarO...7..301W WE94 : Weiss W.W., Paunzen E., Kuschnig R., Schneider H., 1994A&A...281..797W --- Patricia Bauer CDS 1997 Jan 21 Ernst Paunzen <PAUNZEN@astro.ast.univie.ac.at> J_A+AS_123_93.xml An atlas of X- and {gamma}-ray pulse profiles of the Crab pulsar (PSR 0531+21): an analysis of energy and time variations. J/A+AS/124/123 J/A+AS/124/123 Atlas of the Crab pulsar pulse profiles An atlas of X- and {gamma}-ray pulse profiles of the Crab pulsar (PSR 0531+21): an analysis of energy and time variations. E Massaro M Feroci G Matt Astron. Astrophys. Suppl. Ser. 124 123 1997 1997A&AS..124..123M Atlases Pulsars atlases gamma rays: observations pulsars: individual (PSR 0531+21, Crab pulsar) X-rays: stars We present an atlas of X and {gamma}-ray pulse profiles of PSR 0531+21 (Crab pulsar) measured since 1967. This atlas, containing 250 profiles, is useful to study in detail the behaviour with time and energy of this important source and to test models of the emission geometrical pattern. The atlas database is also accessible from Mosaic. An analysis of the energy dependence and time changes of the Crab pulsar light curve (and in particular of the P2/P1 ratio), based on the atlas database, is presented.
PSR 0531+21 Crab pulsar 05 34 31.9 +22 00 52
List of all pulse profiles included in the Atlas Profile Profile --- Epoch1 Epoch of observation or begin of the epoch if interval "DD/MM/YY" --- dash --- Epoch2 End of the epoch of observation "DD/MM/YY" Epocch3 Second epoch of observation "DD/MM/YY" BinN Number of phase bin --- l_Band Limit flag on Band --- Band Lower level of the energy band or upper limit --- --- dash --- Bandu Upper level of the energy band --- n_Band A: average value --- x_Band Units of the energy band --- Max Phase bin of the P1 centre (with the approximation of half a bin) --- Ref References number=2 References: AG90 Agrinier B. et al., 1990ApJ...355..645A AL72 Albats P. et al., 1972Natur.240..221A BC93 Buccheri R. et al., 1993, Adv. Space Res. 13, (12) 727 BD69 Bradt H. et al., 1969Natur.222..728B BF73 Berthelsdorf R. et al., 1973ApL....14..171B BK95 Becker W., Aschenbach B., 1995: in "The lives of Neutron Stars" (A. Alpar, U. Kilizoglu and J. van Paradaijs eds.), Kluwer Acad. Publ. BL69 Boldt E.A. et al., 1969Natur.223..280B BN77 Bennett K. et al., 1977A&A....61..279B BN93 Bennett K. et al., 1993A&AS...97..317B BO72 Boclet D. et al., 1972NPhS..235...69B BR71 Brini D. et al., 1971NPhS..232...79B BT93 Bartlett L.M. et al., 1993, Proc. 2nd Compton Symposium, St. Louis (M. Friedlander, N. Geherels and D.J. Macomb eds.), AIP p. 194 BT94 Bartlett L.M. et al., 1994, Proc. 3rd Compton Symposium, AIP, p.67 BW71 Browning R. Ramsden D., Wright,P.J., 1971NPhS..232...99B CL87 Clear J. et al., 1987A&A...174...85C CN77 Crannell C.J. et al., 1977, Proc. 12th ESLAB Symp. "Recent Advances in Gamma-Ray Astronomy", ESA SP 124, p. 67 CR94 Carraminana A. et al., 1994A&A...290..487C CV71 Cavani C. et al., 1971NPhS..233..153C DB71 Deerenberg A.J.M., Bleeker J.A.M., 1971NPhS..229..113D DC70 Ducros G. et al., 1970Natur.227..152D DV75 Davison P.J.N., 1975MNRAS.173...77D DN92 Denis M., 1992 Ph. D. Thesis Univ. "P. Sabatier", Toulouse FC FIGARO Collaboration (unpublished) FL69 Floyd F.W. et al., 1969Natur.224...50F FR69 Fritz G. et al., 1969Sci...164..709F FR71 Fritz G. et al., 1971ApJ...164L..55F FS69 Fishman G.J., Harnden,F.R., Haymes,R.C., 1969ApJ...156L.107F FS69a Fishman G.J. et al., 1969ApJ...158L..61F FS93 Fishman G.J. et al., 1993A&AS...97...17F GR75 Greisen K. et al., 1975ApJ...197..471G GS82 Graser U., Schonfelder V., 1982ApJ...263..677G HG82 Hasinger G., 1982, in "Accreting Neutron Stars" (W. Brinkmann and J. Trumper eds.), MPE report 177, p. 130 HG84 Hasinger G., 1984. Proc. Int. Symp. on X-ray Astronomy, Bologna 1983, p. 321 HL70 Hillier R.R. et al., 1970ApJ...162L.177H HM83 Hameury J.M. et al., 1983ApJ...270..144H HM83 Harnden F.R., 1983. Proc. IAU Symp. "Supernova Remnants and their X-Ray Emission" (J. Danzinger and P. Gorenstein eds.), p. 131 HR94 Hermsen W. et al., 1994ApJS...92..559H HS84 Harnden F.R., Seward F.D., 1984ApJ...283..279H KB77 Kanbach G. et al., 1977, Proc. 12th ESLAB Symp. "Recent Advances in Gamma-Ray Astronomy", ESA SP 124, p. 21 KF71 Kurfess J.D., 1971ApJ...168L..39K KG82 Knight F.K., 1982ApJ...260..538K KN74 Kniffen D.A. et al., 1974Natur.251..397K KS76 Kestenbaum H.L. et al., 1976ApJ...203L..57K KT71 Kettenring G. et al., 1971, Proc. 12th ICRC, Hobart OG 16 KU86 Kurt V.G. et al., 1986SvA....30..560K KW93 Kawai N., Okayasu R., Sekimoto Y., 1993, Proc. 2nd Compton Symposium, St. Louis (M. Friedlander, N. Geherels and D.J. Macomb eds.), AIP p. 213 KZ71 Kinzer R.L. et al., 1971Natur.229..187K KZ73 Kinzer R.L., Share G.H., Seeman N., 1973ApJ...180..547K LR72 Leray J.P. et al., 1972A&A....16..443L LS73 Laros J.G. et al., 1973NPhS..246..109L MB73 McBreen B. et al., 1973ApJ...184..571M MC94 Much R.P., 1994, Ph.D. Thesis MPE Report 251 MC95 Much R.P. et al., 1995A&A...299..435M MC95a Much R.P. et al., 1995, Adv. Space Res. 15, 81 MH84 Mahoney W.A. et al., 1984ApJ...278..784M MN94 Masnou J.L. et al., 1994A&A...290..503M MS91 Massaro E. et al., 1991ApJ...376L..11M MS91a Massaro E. et al., 1991, Proc. 22nd ICRC, 1, 181 NG94 Nagase F., Zylstra G., Mihara T.: 1994, "New Horizon of X-Ray Astronomy", (F. Makino and T.Ohashi eds.) Proc. Int. Conf., Tokyo March 8-11, 1994, p. 57 NL93 Nolan P.L et al., 1993ApJ...409..697N NT91 Natalucci L. et al., 1991, Adv. Space. Res. 11, (8) 79 OR71 Orwig L.E. et al., 1971NPhS..231..171O PL73 Parlier B. et al., 1973NPhS..242..117P PR81 Pravdo S.H., Serlemitsos P.J., 1981ApJ...246..484P RC77 Ryckman S.G. et al., 197NPhS..266..431R ] RM95 Ramanamurthy P.V. et al., 1995ApJ...450..791R RP71 Rappaport S. et al., 1971NPhS..229...38R SM71 Smathers H.W. et al., 1971NPhS..232..120S ST79 Strickman M.S., Johnson W.N., Kurfess J.D., 1979ApJ...230L..15S ST82 Strickman M.S., Kurfess J.D., Johnson W.N., 1982ApJ...253L..23S TH71 Tuohy I.R. et al., 1971, Proc. 12th ICRC, Hobart OG 4, p. 13 TM77 Thompson D.J. et al., 1977ApJ...213..252T TM93 Thompson D.J. et al., 1993, in "Isolated Pulsars" (K.A. van Riper, R. Epstein and C. Ho eds.), Cambridge Univ. Press, p. 230 TS77 Toor A., Seward F., 1977ApJ...216..560T UB94 Ubertini P. et al., 1994ApJ...421..269U UL92 Ulmer M.P. et al., 1992, Proc. 1st Compton Symp., Annapolis, 23-25 Sept. 1991, (C.R. Shrader, N. Gehrels, B. Dennis eds.), NASA Conf. Publ. 3137, p. 253 UL94 Ulmer M.P. et al., 1994ApJ...432..228U UL94a Ulmer M.P., 1994ApJS...90..789U UL95 Ulmer M.P. et al., 1995ApJ...448..356U VS70 Vasseur J. et al., 1970Natur.226..534V VS71 Vasseur J. et al., 1971NPhS..233...46V WF83 Wilson R.B., Fishman G.J., 1983ApJ...269..273W WH85 White R.S. et al., 1985ApJ...299L..23W WK78 Weisskopf M.C. et al., 1978ApJ...220L.117W WL81 Wills R.D. et al., 1981, Phil. Trans. R. Soc. London A301, 537 WL82 Wills R.D. et al., 1982Natur.296..723W WR75 Walraven G.D. et al., 1975ApJ...202..502W WS93 Wilson R.B. et al., 1993, in "Isolated Pulsars" (K.A. van Riper, R. Epstein and C. Ho eds.), Cambridge Univ. Press, p. 257 --- Note Note number=1 1: In the original paper the size of P1 bins is 1/2 of the other bins. Here the counts in P1 were binned two by two to have the same binning trough all the profile. 2: In the original paper the pulse profile has 199 bins instead of the 200 quoted in the text. No additional bin has been added in the profile of the atlas. 3: In the original paper the pulse profile has 65 bins instead of the 66 quoted in the text. An additional bin has been added in the profile of the atlas with a count rate equal to that of the off-pulse level. 4: This pulse profile is not included in the original paper but was computed by adding the four profiles from HX 08_1 to HX 08_4. 5: The precise epoch of each pulse profile is not explicitly specified in the paper 6: Sum of the pulse profiles HX 20_1, HX 27_1 and HX 28_1, reported in the quoted reference. 7: This pulse profile is not included in the original paper but was computed by adding the two profiles HG 19_1 and HG 19_2. 8: This pulse profile is not included in the original paper but was computed by adding the four profiles from HG 19_4 to HG 19_7. --- Patricia Bauer CDS 1997 Apr 25 Enrico Massaro <massaro@astrm2.rm.astro.it> J_A+AS_124_123.xml UBVRI imaging photometry of the open cluster Cr 272 J/A+AS/124/13 J/A+AS/124/13 UBVRI photometry of the cluster Collinder 272 UBVRI imaging photometry of the open cluster Cr 272 R A Vazquez G Baume A Feinstein P Prado Astron. Astrophys. Suppl. Ser. 124 13 1997 1997A&AS..124...13V Clusters, open Photometry, UBVRI Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Cr 272) stars: luminosity function, mass function We present an extensive CCD UBVRI (Cousins system) photometric survey in the region of the open cluster Collinder 272. Our data analysis confirms that the cluster is situated in the outer border of Becker's inner arm -II, at a distance d=2300pc and probably related to the neighbor cluster Hogg 16. There is no highly evolved stars in the cluster upper sequence and our age estimate based upon isochrones from models computed with mass loss and overshooting, and other methods, indicates a mean age of 13Myr. A statistical method based on the removal of field stars was used to determine the luminosity function and the initial mass function of the cluster. The cluster initial mass function is characterized by a slope x=1.8.
Cr 272 Collinder 272 C 1327-610 13 30.6 -61 16
CCD photometric observations in Cr272 No Sequence number --- Xpos X position pix Ypos Y position pix Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- B-V B-V color index mag u_B-V Uncertainty flag on B-V number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- U-B U-B color index mag u_U-B Uncertainty flag on U-B number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- V-R V-R color index mag u_V-R Uncertainty flag on V-R number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- V-I V-I color index mag u_V-I Uncertainty flag on V-I number=1 (:) errors larger than 0.04 (::) errors larger than 0.08 --- Rem Remark number=2 lm = likely member pm = probable member --- table2.tex LaTeX version of Table 2 Ruben Vazquez Observ. Astron. La Plata 1997 Jan 17 Ruben Vazquez <rvazquez@fcaglp.fcaglp.unlp.edu.ar> J_A+AS_124_13.xml Mean light curves of long-period variables and discrimination between carbon- and oxygen-rich stars. J/A+AS/124/143 J/A+AS/124/143 Light curves of O and C-rich LPV's Mean light curves of long-period variables and discrimination between carbon- and oxygen-rich stars. M O Mennessier H Boughaleb J A Mattei Astron. Astrophys. Suppl. Ser. 124 143 1997 1997A&AS..124..143M Stars, variable methods: data analysis stars: AGB and post-AGB stars: carbon stars: variables: other Mira and semiregular variables: mean parameters of light curves from 75 years AAVSO data.
Mean light curve parameters Name Star name from GCVS (Cat. <II/172>) --- o_Per Number of periods --- o_Max Number of maxima --- o_Min Number of minima --- o_Amp Number of amplitudes --- Per Mean period number=1 According to the available data, the period of R Aql has decreased from 334 to 278 days over a 73 years interval d F Mean asymmetry factor number=2 Asymmetry factor: ratio of the increasing time (from minimum to the following maximum) to the period --- Max Mean magnitude at maximum mag Min Mean magnitude at minimum mag Amp Mean visual amplitude mag e_Per Standard deviation of periods d e_F Standard deviation of asymmetry factors --- e_Max Standard deviation of maximum magnitudes mag e_Min Standard deviation of minimum magnitudes mag e_Amp Standard deviation of amplitudes mag Vtype Variability type (GCVS, Cat. <II/172>) --- SpType Brief spectral type (GCVS, Cat. <II/172>) --- Patricia Bauer CDS 1996 Nov 25 Marie Odile Menessier <menes@graal1.graal.univ-montp2.fr> J_A+AS_124_143.xml Absolute proper motions for the calibration of the Hipparcos proper motion system J/A+AS/124/157 J/A+AS/124/157 Hipparcos stars proper motions Absolute proper motions for the calibration of the Hipparcos proper motion system M Geffert A R Klemola M Hiesgen J Schmoll Astron. Astrophys. Suppl. Ser. 124 157 1997 1997A&AS..124..157G Proper motions astrometry reference systems stars: kinematics Absolute proper motions of 48 Hipparcos stars in nine fields distributed over the northern hemisphere are presented. The proper motions have been recently used as part of the Bonn program for the extragalactic link of the Hipparcos proper motion system. We describe methods which have led to the absolute proper motions of the major part of the Bonn fields for the link. For six fields the extragalactic calibration was achieved using the bright quasar in the centre of the field. In addition, data of three fields of globular clusters were included. For these fields the link to an extragalactic reference system was performed by stars, whose absolute proper motions with respect to galaxies were determined on plates of the Lick astrograph. In addition, we used for the link in one field plates from the ESO Schmidt telescope in combination with measurements from glass copies of the Palomar Sky Survey. The accuracy of a single proper motion is of the order of 2 to 3mas/a for each coordinate.
48 stars with absolute proper motion for the calibration of the Hipparcos proper motion system. The epoch of the observations is 1950. Name Star name --- HIC HIC (Hipparcos Input Catalogue <I/196>) number --- RAh Right ascension (Eq=J2000, Ep=1950) h RAm Right ascension (Eq=J2000, Ep=1950) min RAs Right ascension (Eq=J2000, Ep=1950) s DE- Declination sign --- DEd Declination (Eq=J2000, Ep=1950) deg DEm Declination (Eq=J2000, Ep=1950) arcmin DEs Declination (Eq=J2000, Ep=1950) arcsec pmRA Proper motion in right ascension (mu_alpha_cos(delta)) number=1 The internal accuracy of the proper motions is of the order of 2mas/a. mas/a pmDE Proper motion in declination (mu_delta_) number=1 The internal accuracy of the proper motions is of the order of 2mas/a. mas/a table2.tex LaTeX version of table2 Patricia Bauer CDS 1996 Nov 12 J_A+AS_124_157.xml Studies of the Centaurus cluster. I. A catalogue of galaxies in the central region of the Centaurus cluster J/A+AS/124/1 J/A+AS/124/1 The Centaurus Cluster Catalogue Studies of the Centaurus cluster. I. A catalogue of galaxies in the central region of the Centaurus cluster H Jerjen A Dressler Astron. Astrophys. Suppl. Ser. 124 1 1997 1997A&AS..124....1J Clusters, galaxy Galaxies, photometry catalogs galaxies: clusters: individual (Centarus cluster) galaxies: fundamental parameters galaxies: photometry The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.
The Centaurus Cluster Catalogue CCC Catalogue Number --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec MType Morphological type --- Class Cluster membership (1=100%, 2=75%, 3=50%) --- BT Total apparent B magnitude mag Q Quality of the derived growth curves number=1 Quality parameter: 1=very, 2=good, 3=fair, 4=poor --- SBe Mean effective surface brightness mag/arcsec2 log(Re) Logarithm of the effective radius arcsec mu0 Central exp surface brightness number=2 Data resulting from the best fit of an exponential law [mu(r)=mu0+1.086*(r/a)] at the observed surface brightness profile mag/arcsec2 log(a) Logarithm of the exp scale length number=2 Data resulting from the best fit of an exponential law [mu(r)=mu0+1.086*(r/a)] at the observed surface brightness profile arcsec N Exponent of the generalized exp profile number=2 Data resulting from the best fit of an exponential law [mu(r)=mu0+1.086*(r/a)] at the observed surface brightness profile --- HRV Heliocentric radial velocity km/s r_HRV Reference code for HRV see note number=3 1: Dickens et al., 1986MNRAS.220..679D 2: Lucey & Carter, 1988MNRAS.235.1177L 3: Stein 1994, PhD Thesis, University of Basel --- Name Other names see note number=4 B: Bothun et al., 1989AJ.....98.1542B D: Dressler 1980, Cat. <VII/174> DCL: Dickens et al., 1986MNRAS.220..679D 6 digit number: Lauberts, 1982ESO...C......0L --- Patricia Bauer CDS 1996 Nov 12 Helmut Jerjen <jerjen@mso.anu.edu.au> J_A+AS_124_1.xml Physical and chemical variations within the W 3 star-forming region. II. The 345 GHz spectral line survey J/A+AS/124/205 J/A+AS/124/205 W3 star-forming region 345 GHz survey Physical and chemical variations within the W 3 star-forming region. II. The 345 GHz spectral line survey F P Helmich E F Van Dishoeck Astron. Astrophys. Suppl. Ser. 124 205 1997 1997A&AS..124..205H Infrared sources Interstellar medium Radio lines ISM: clouds ISM: individual (W 3 IRS5, W 3IRS4, W 3H2O) ISM: molecules radio lines: ISM surveys Results are presented of the 345 GHz spectral survey toward three sources in the W 3 Giant Molecular Cloud: W 3 IRS4, W 3 IRS5 and W 3(H_2_O). Nearly 90% of the atmospheric window between 334 and 365GHz has been scanned using the James Clerk Maxwell Telescope (JCMT) down to a noise level of ~80mK per resolution element. These observations are complemented by a large amount of data in the 230GHz atmospheric window. From this data set physical conditions and beam-averaged column densities are derived for more than 14 chemically different species (over 24 different isotopes). The physical parameters derived in Paper I (Helmich et al., 1994A&A...283..626H) are confirmed by the analysis of the excitation of other species, although there is evidence that the silicon- and sulfur-bearing molecules exist in a somewhat denser and warmer environment. The densities are high, >=10^6^cm^-3^, in the three sources and the kinetic temperatures for the bulk of the gas range from 55K for IRS4 to 220K for W 3(H_2_O). The chemical differences between the three sources are very striking: silicon- and sulfur-bearing molecules such as SiO and SO_2_ are prominent toward IRS5, whereas organic molecules like CH_3_OH, CH_3_OCH_3_ and CH_3_OCHO are at least an order of magnitude more abundant toward W 3(H_2_O). Vibrationally excited molecules are also detected toward this source. Only simple molecules are found toward IRS4. The data provide constraints on the amount of deuterium fractionation and the ionization fraction in the observed regions as well. These chemical characteristics are discussed in the context of an evolutionary sequence, in which IRS5 is the youngest, W 3(H_2_O) somewhat older and IRS4, although still enigmatic, the oldest.
W 3 IRS 4 02 25 30.8 +62 06 21 W 3 IRS 5 02 25 40.6 +62 05 52 W 3 (H2O) 02 27 04.6 +61 52 25
*Gaussian fit parameters Species Species --- n_Species Note on species number=2 1: Gaussian decomposition not unique because of selfreversed profile and strong wings, only integral under line given. 2: Distorted profile, cause unknown. 3: Gaussian decomposition not unique because of strong wings, only peak temperature given. 4: The {DELTA}V is kept fixed in the Gaussian fit. 5: On edge of spectrum. 6: Bad base line. 7: Line offset by 3 MHz, incorrect identification? a: Blended with CH_3_OCH_3_ 339491. b: Blended with C^34^S 7--6. c: H^13^CN 4--3 always blended with SO_2_ 345338. d: HC^15^N 3--2 blended with CH_3_OCH_3_ 260754/56/58/61. e: HNC 4--3 blended with SO_2_ 359770. f: HN^13^C 3--2 blended with SO_2_ 258666. g: Blended with CH_3_OCH_3_ 358447-358456. h: In wing SO_2_ 351257. i: H_2_CS 244047 blended with HNCO 240875/6. j: CH_3_CCH 358818 blended with CH_3_CCH 358811. k: Uncertain, could also be a base-line ripple l: H_2_CO 5_42_-4_41_ and 5_41_-4_40_ are always blended. m: H_2_CO 364289 blended with CH_3_OH 360849. n: Blended with H_2_CS and CN. o: H_2_^13^CO 354898 blended with SO_2_ 358013. p: H_2_^13^CO 355041 blended with SO_2_ 355045. q: CH_3_CN 257507/22/27 blended with CH_3_OCHO 260384/392 /404/415. r: CH_3_CN 257522 blended with CH_3_OCH_3_ 260400/1/3/5 s: Blended with CCH 349337/8. t: CH_3_CN 349446 blended with CH_3_CN 349453. u: Blended with CH_3_OH 243915. v: SO 346528 always blended with SO_2_ 346523. w: ^34^SO 337582 blended with CH_3_OH 337581. x: Large frequency error in line catalogues. y: Four hyperfine components of ^33^SO blended with CH_3_OH 337198. z: Blended with CH_3_OH 7_K_-6_K_ band. aa: SO 219949 Slightly blended with SO_2_ 222689. ab: SO_2_ 254280 blended with SO_2_ 254283 and ^34^SO_2_ 254278. ac: SO_2_ 258667 blended with CH_3_OCH_3_ 261245/46/48/50. ad: CH_3_OH 338615 blended with SO_2_ 338611 and SO_2_ 335773. ae: CH_3_OH 338615 blended with SO_2_ 338611. af: SO_2_ 346652 blended with CH_3_OH 349845. ag: SO_2_ 363925 blended with CH_3_OH 361236. ah: ^34^SO_2_ 243935 blended with CH_3_OCH_3_ 240978/82/85/89. ai: ^34^SO_2_ 260327 blended with CH_3_OCH_3_ 26027/29/31. aj: ^34^SO_2_ 342231 blended with ^34^SO_2_ 345678. ak: ^34^SO_2_ 348117 blended with ^34^SO_2_ 345519. al: ^34^SO_2_ 358988 blended with ^34^SO_2_ 355920. am: ^34^SO_2_ 358988 blended with DCN 5--4 362046. an: HCN {upsilon}_2_ 356255.6 blended with ^34^SO_2_ 359651. ao: Blended with H_2_^13^CO 343325. ap: H_2_CS 343408 blended with H_2_CS 343412. aq: OCS 30-29 blended with CH_3_OH 364746 and CH_3_OH 364757. ar: Blended with CH_3_CN 14_5_--13_5_ and CH_3_OH 257402. as: HCS^+^ 8--7 blended with CH_3_OCHO 344539. --- nu Frequency MHz J Transition designation --- l_TMBa Limit flag on TMBa number=1 All upper limits are 2 times the rms noise in one resolution element (generally two channels). --- TMBa W3 IRS4 temperature K n_TMBa Note on TMBa number=2 1: Gaussian decomposition not unique because of selfreversed profile and strong wings, only integral under line given. 2: Distorted profile, cause unknown. 3: Gaussian decomposition not unique because of strong wings, only peak temperature given. 4: The {DELTA}V is kept fixed in the Gaussian fit. 5: On edge of spectrum. 6: Bad base line. 7: Line offset by 3 MHz, incorrect identification? a: Blended with CH_3_OCH_3_ 339491. b: Blended with C^34^S 7--6. c: H^13^CN 4--3 always blended with SO_2_ 345338. d: HC^15^N 3--2 blended with CH_3_OCH_3_ 260754/56/58/61. e: HNC 4--3 blended with SO_2_ 359770. f: HN^13^C 3--2 blended with SO_2_ 258666. g: Blended with CH_3_OCH_3_ 358447-358456. h: In wing SO_2_ 351257. i: H_2_CS 244047 blended with HNCO 240875/6. j: CH_3_CCH 358818 blended with CH_3_CCH 358811. k: Uncertain, could also be a base-line ripple l: H_2_CO 5_42_-4_41_ and 5_41_-4_40_ are always blended. m: H_2_CO 364289 blended with CH_3_OH 360849. n: Blended with H_2_CS and CN. o: H_2_^13^CO 354898 blended with SO_2_ 358013. p: H_2_^13^CO 355041 blended with SO_2_ 355045. q: CH_3_CN 257507/22/27 blended with CH_3_OCHO 260384/392 /404/415. r: CH_3_CN 257522 blended with CH_3_OCH_3_ 260400/1/3/5 s: Blended with CCH 349337/8. t: CH_3_CN 349446 blended with CH_3_CN 349453. u: Blended with CH_3_OH 243915. v: SO 346528 always blended with SO_2_ 346523. w: ^34^SO 337582 blended with CH_3_OH 337581. x: Large frequency error in line catalogues. y: Four hyperfine components of ^33^SO blended with CH_3_OH 337198. z: Blended with CH_3_OH 7_K_-6_K_ band. aa: SO 219949 Slightly blended with SO_2_ 222689. ab: SO_2_ 254280 blended with SO_2_ 254283 and ^34^SO_2_ 254278. ac: SO_2_ 258667 blended with CH_3_OCH_3_ 261245/46/48/50. ad: CH_3_OH 338615 blended with SO_2_ 338611 and SO_2_ 335773. ae: CH_3_OH 338615 blended with SO_2_ 338611. af: SO_2_ 346652 blended with CH_3_OH 349845. ag: SO_2_ 363925 blended with CH_3_OH 361236. ah: ^34^SO_2_ 243935 blended with CH_3_OCH_3_ 240978/82/85/89. ai: ^34^SO_2_ 260327 blended with CH_3_OCH_3_ 26027/29/31. aj: ^34^SO_2_ 342231 blended with ^34^SO_2_ 345678. ak: ^34^SO_2_ 348117 blended with ^34^SO_2_ 345519. al: ^34^SO_2_ 358988 blended with ^34^SO_2_ 355920. am: ^34^SO_2_ 358988 blended with DCN 5--4 362046. an: HCN {upsilon}_2_ 356255.6 blended with ^34^SO_2_ 359651. ao: Blended with H_2_^13^CO 343325. ap: H_2_CS 343408 blended with H_2_CS 343412. aq: OCS 30-29 blended with CH_3_OH 364746 and CH_3_OH 364757. ar: Blended with CH_3_CN 14_5_--13_5_ and CH_3_OH 257402. as: HCS^+^ 8--7 blended with CH_3_OCHO 344539. --- DVa W3 IRS4 {DELTA}V km/s Wa W3 IRS4 integrated intensity K.km/s l_TMBb Limit flag on TMBb number=1 All upper limits are 2 times the rms noise in one resolution element (generally two channels). --- TMBb W3 IRS5 temperature K n_TMBb Note on TMBb number=2 1: Gaussian decomposition not unique because of selfreversed profile and strong wings, only integral under line given. 2: Distorted profile, cause unknown. 3: Gaussian decomposition not unique because of strong wings, only peak temperature given. 4: The {DELTA}V is kept fixed in the Gaussian fit. 5: On edge of spectrum. 6: Bad base line. 7: Line offset by 3 MHz, incorrect identification? a: Blended with CH_3_OCH_3_ 339491. b: Blended with C^34^S 7--6. c: H^13^CN 4--3 always blended with SO_2_ 345338. d: HC^15^N 3--2 blended with CH_3_OCH_3_ 260754/56/58/61. e: HNC 4--3 blended with SO_2_ 359770. f: HN^13^C 3--2 blended with SO_2_ 258666. g: Blended with CH_3_OCH_3_ 358447-358456. h: In wing SO_2_ 351257. i: H_2_CS 244047 blended with HNCO 240875/6. j: CH_3_CCH 358818 blended with CH_3_CCH 358811. k: Uncertain, could also be a base-line ripple l: H_2_CO 5_42_-4_41_ and 5_41_-4_40_ are always blended. m: H_2_CO 364289 blended with CH_3_OH 360849. n: Blended with H_2_CS and CN. o: H_2_^13^CO 354898 blended with SO_2_ 358013. p: H_2_^13^CO 355041 blended with SO_2_ 355045. q: CH_3_CN 257507/22/27 blended with CH_3_OCHO 260384/392 /404/415. r: CH_3_CN 257522 blended with CH_3_OCH_3_ 260400/1/3/5 s: Blended with CCH 349337/8. t: CH_3_CN 349446 blended with CH_3_CN 349453. u: Blended with CH_3_OH 243915. v: SO 346528 always blended with SO_2_ 346523. w: ^34^SO 337582 blended with CH_3_OH 337581. x: Large frequency error in line catalogues. y: Four hyperfine components of ^33^SO blended with CH_3_OH 337198. z: Blended with CH_3_OH 7_K_-6_K_ band. aa: SO 219949 Slightly blended with SO_2_ 222689. ab: SO_2_ 254280 blended with SO_2_ 254283 and ^34^SO_2_ 254278. ac: SO_2_ 258667 blended with CH_3_OCH_3_ 261245/46/48/50. ad: CH_3_OH 338615 blended with SO_2_ 338611 and SO_2_ 335773. ae: CH_3_OH 338615 blended with SO_2_ 338611. af: SO_2_ 346652 blended with CH_3_OH 349845. ag: SO_2_ 363925 blended with CH_3_OH 361236. ah: ^34^SO_2_ 243935 blended with CH_3_OCH_3_ 240978/82/85/89. ai: ^34^SO_2_ 260327 blended with CH_3_OCH_3_ 26027/29/31. aj: ^34^SO_2_ 342231 blended with ^34^SO_2_ 345678. ak: ^34^SO_2_ 348117 blended with ^34^SO_2_ 345519. al: ^34^SO_2_ 358988 blended with ^34^SO_2_ 355920. am: ^34^SO_2_ 358988 blended with DCN 5--4 362046. an: HCN {upsilon}_2_ 356255.6 blended with ^34^SO_2_ 359651. ao: Blended with H_2_^13^CO 343325. ap: H_2_CS 343408 blended with H_2_CS 343412. aq: OCS 30-29 blended with CH_3_OH 364746 and CH_3_OH 364757. ar: Blended with CH_3_CN 14_5_--13_5_ and CH_3_OH 257402. as: HCS^+^ 8--7 blended with CH_3_OCHO 344539. --- DVb W3 IRS5 {DELTA}V km/s Wb W3 IRS5 integrated intensity K.km/s l_TMBc Limit flag on TMBc number=1 All upper limits are 2 times the rms noise in one resolution element (generally two channels). --- TMBc W3 (H2O) temperature K n_TMBc Note on TMBa number=2 1: Gaussian decomposition not unique because of selfreversed profile and strong wings, only integral under line given. 2: Distorted profile, cause unknown. 3: Gaussian decomposition not unique because of strong wings, only peak temperature given. 4: The {DELTA}V is kept fixed in the Gaussian fit. 5: On edge of spectrum. 6: Bad base line. 7: Line offset by 3 MHz, incorrect identification? a: Blended with CH_3_OCH_3_ 339491. b: Blended with C^34^S 7--6. c: H^13^CN 4--3 always blended with SO_2_ 345338. d: HC^15^N 3--2 blended with CH_3_OCH_3_ 260754/56/58/61. e: HNC 4--3 blended with SO_2_ 359770. f: HN^13^C 3--2 blended with SO_2_ 258666. g: Blended with CH_3_OCH_3_ 358447-358456. h: In wing SO_2_ 351257. i: H_2_CS 244047 blended with HNCO 240875/6. j: CH_3_CCH 358818 blended with CH_3_CCH 358811. k: Uncertain, could also be a base-line ripple l: H_2_CO 5_42_-4_41_ and 5_41_-4_40_ are always blended. m: H_2_CO 364289 blended with CH_3_OH 360849. n: Blended with H_2_CS and CN. o: H_2_^13^CO 354898 blended with SO_2_ 358013. p: H_2_^13^CO 355041 blended with SO_2_ 355045. q: CH_3_CN 257507/22/27 blended with CH_3_OCHO 260384/392 /404/415. r: CH_3_CN 257522 blended with CH_3_OCH_3_ 260400/1/3/5 s: Blended with CCH 349337/8. t: CH_3_CN 349446 blended with CH_3_CN 349453. u: Blended with CH_3_OH 243915. v: SO 346528 always blended with SO_2_ 346523. w: ^34^SO 337582 blended with CH_3_OH 337581. x: Large frequency error in line catalogues. y: Four hyperfine components of ^33^SO blended with CH_3_OH 337198. z: Blended with CH_3_OH 7_K_-6_K_ band. aa: SO 219949 Slightly blended with SO_2_ 222689. ab: SO_2_ 254280 blended with SO_2_ 254283 and ^34^SO_2_ 254278. ac: SO_2_ 258667 blended with CH_3_OCH_3_ 261245/46/48/50. ad: CH_3_OH 338615 blended with SO_2_ 338611 and SO_2_ 335773. ae: CH_3_OH 338615 blended with SO_2_ 338611. af: SO_2_ 346652 blended with CH_3_OH 349845. ag: SO_2_ 363925 blended with CH_3_OH 361236. ah: ^34^SO_2_ 243935 blended with CH_3_OCH_3_ 240978/82/85/89. ai: ^34^SO_2_ 260327 blended with CH_3_OCH_3_ 26027/29/31. aj: ^34^SO_2_ 342231 blended with ^34^SO_2_ 345678. ak: ^34^SO_2_ 348117 blended with ^34^SO_2_ 345519. al: ^34^SO_2_ 358988 blended with ^34^SO_2_ 355920. am: ^34^SO_2_ 358988 blended with DCN 5--4 362046. an: HCN {upsilon}_2_ 356255.6 blended with ^34^SO_2_ 359651. ao: Blended with H_2_^13^CO 343325. ap: H_2_CS 343408 blended with H_2_CS 343412. aq: OCS 30-29 blended with CH_3_OH 364746 and CH_3_OH 364757. ar: Blended with CH_3_CN 14_5_--13_5_ and CH_3_OH 257402. as: HCS^+^ 8--7 blended with CH_3_OCHO 344539. --- DVc W3 (H2O) {DELTA}V km/s n_DVc Note on DVc number=2 1: Gaussian decomposition not unique because of selfreversed profile and strong wings, only integral under line given. 2: Distorted profile, cause unknown. 3: Gaussian decomposition not unique because of strong wings, only peak temperature given. 4: The {DELTA}V is kept fixed in the Gaussian fit. 5: On edge of spectrum. 6: Bad base line. 7: Line offset by 3 MHz, incorrect identification? a: Blended with CH_3_OCH_3_ 339491. b: Blended with C^34^S 7--6. c: H^13^CN 4--3 always blended with SO_2_ 345338. d: HC^15^N 3--2 blended with CH_3_OCH_3_ 260754/56/58/61. e: HNC 4--3 blended with SO_2_ 359770. f: HN^13^C 3--2 blended with SO_2_ 258666. g: Blended with CH_3_OCH_3_ 358447-358456. h: In wing SO_2_ 351257. i: H_2_CS 244047 blended with HNCO 240875/6. j: CH_3_CCH 358818 blended with CH_3_CCH 358811. k: Uncertain, could also be a base-line ripple l: H_2_CO 5_42_-4_41_ and 5_41_-4_40_ are always blended. m: H_2_CO 364289 blended with CH_3_OH 360849. n: Blended with H_2_CS and CN. o: H_2_^13^CO 354898 blended with SO_2_ 358013. p: H_2_^13^CO 355041 blended with SO_2_ 355045. q: CH_3_CN 257507/22/27 blended with CH_3_OCHO 260384/392 /404/415. r: CH_3_CN 257522 blended with CH_3_OCH_3_ 260400/1/3/5 s: Blended with CCH 349337/8. t: CH_3_CN 349446 blended with CH_3_CN 349453. u: Blended with CH_3_OH 243915. v: SO 346528 always blended with SO_2_ 346523. w: ^34^SO 337582 blended with CH_3_OH 337581. x: Large frequency error in line catalogues. y: Four hyperfine components of ^33^SO blended with CH_3_OH 337198. z: Blended with CH_3_OH 7_K_-6_K_ band. aa: SO 219949 Slightly blended with SO_2_ 222689. ab: SO_2_ 254280 blended with SO_2_ 254283 and ^34^SO_2_ 254278. ac: SO_2_ 258667 blended with CH_3_OCH_3_ 261245/46/48/50. ad: CH_3_OH 338615 blended with SO_2_ 338611 and SO_2_ 335773. ae: CH_3_OH 338615 blended with SO_2_ 338611. af: SO_2_ 346652 blended with CH_3_OH 349845. ag: SO_2_ 363925 blended with CH_3_OH 361236. ah: ^34^SO_2_ 243935 blended with CH_3_OCH_3_ 240978/82/85/89. ai: ^34^SO_2_ 260327 blended with CH_3_OCH_3_ 26027/29/31. aj: ^34^SO_2_ 342231 blended with ^34^SO_2_ 345678. ak: ^34^SO_2_ 348117 blended with ^34^SO_2_ 345519. al: ^34^SO_2_ 358988 blended with ^34^SO_2_ 355920. am: ^34^SO_2_ 358988 blended with DCN 5--4 362046. an: HCN {upsilon}_2_ 356255.6 blended with ^34^SO_2_ 359651. ao: Blended with H_2_^13^CO 343325. ap: H_2_CS 343408 blended with H_2_CS 343412. aq: OCS 30-29 blended with CH_3_OH 364746 and CH_3_OH 364757. ar: Blended with CH_3_CN 14_5_--13_5_ and CH_3_OH 257402. as: HCS^+^ 8--7 blended with CH_3_OCHO 344539. --- Wc W3 (H2O) integrated intensity K.km/s CH_3_OH Gaussian fit parameters W 3 IRS4 CH_3_OH Gaussian fit parameters W 3 IRS5 nu Frequency MHz NJ Transition designation --- TMB Temperature K n_TMB Note number=1 1: On edge of spectrum 2: Bad base line 3: CH_3_OH 360849 slightly blended with H_2_CO 364289 a: Blended with ^34^SO 337582 b: Not a certain detection c: CH_3_OH 338615 blended with SO_2_ 338611 --- DV {DELTA}V km/s W Integrated intensity K.km/s CH_3_OH Gaussian fit parameters W 3(H_2_O) nut Quantum number of the torsional mode --- nu Frequency MHz NJ Transition designation --- l_TMB Limit flag on TMB number=1 All upper limits are 2 times the rms noise in one resolution element (generally two channels) --- TMB Temperature K n_TMB Note number=2 1: Strange profile 2: On edge of spectrum a: Blended with ^13^CO 2--1 b: CH_3_OH 241791 blended with CH_3_OH 244330 c: CH_3_OH 241829 blended with CH_3_CN 239096 d: CH_3_OH 241904 blended with CH_3_CN 239022 and CH_3_OCH_3_ 239020/1 e: CH_3_OH 241590 blended with CH_3_OH 244338 and CH_3_OH 244330 f: CH_3_OH 257402 blended with CH3CN 257403 and SiO 6-5 g: CH_3_OH 260381 blended with CH_3_OCHO 260384 h: CH_3_OH 337135 blended with CN 340261 i: CH_3_OH 338615 blended with SO_2_ 338611 j: CH_3_OH 340141 blended with CH_3_OCHO 343435/43 k: CH_3_OH 360849 blended with H_2_CO 364289 l: CH_3_OH 334426 blended with CH_3_OH 337312 m: CH_3_OH 337295 blended with CH_3_OH 337297 n: CH_3_OH 337707 blended with CH_3_OCH_3_ 337708/12 o: CH_3_OH 349845 blended with SO_2_ 346652 p: CH_3_OH 359676 blended with H_2_CO 362735 q: CH_3_OH 361237 blended with SO_2_ 363890 r: CH_3_OH 361852 and CH_3_OH 364508 blended with CH_3_OCH_3_ 361863 and CH_3_OCH_3_ 361871/4/7 s: CH_3_OH 364757 blended with CH_3_OH 364746 and OCS 30-29 t: CH_3_OH 337198 blended with ^33^SO 337198 u: CH_3_OH 337252 blended with CH_3_OH 340141 --- DV {DELTA}V km/s W Integrated intensity K.km/s CH_3_OCH_3_ Gaussian fit parameters W 3(H_2_O) nu Frequency MHz Jk J_k_0_,k_p__ transition designation --- l_TMB Limit flag on TMB --- TMB Temperature K n_TMB Note number=1 1: On edge of spectrum 2: Bad base line a: CH_3_OCH_3_ 239020/1 blended with CH_3_OH 241904 and CH_3_CN 239022 b: CH_3_OCH_3_ 241523/28/30 blended with CH_3_OCHO 244594 c: CH_3_OCH_3_ 241635/7/8 may be AOS spike d: CH_3_OCH_3_ 244503/08/12 blended with SO_2_ 241615 e: CH_3_OCH_3_ 260400/1/3/5 thoroughly blended with CH_3_CN257522 and CH_3_OCHO 260392/404 f: CH_3_OCH_3_ 260754/56/58/61 blended with HC^15^N 3--2 g: CH_3_OCH_3_ 261145/47/48/50 blended with CH_3_OCHO 261148 h: CH_3_OCH_3_ 261245/46/48/50 blended with SO_2_ 258666 i: CH_3_OCH_3_ 339491 blended with CN 339493 j: CH_3_OCH_3_ 342608 blended with ^34^SO_2_ 345285 k: CH_3_OCH_3_ 356705/12/16/23/24 on wing of HCO^+^ 4--3 l: CH_3_OCH_3_ 361863 and CH_3_OCH_3_ 361871/4/7 blended with CH_3_OH 361852 and CH_3_OH 364508. --- DV {DELTA}V km/s W Integrated intensity K.km/s CH_3_OCHO Gaussian fit parameters W 3(H_2_O) nu Frequency MHz J Transition designation --- l_TMB Limit flag on TMB --- TMB Temperature K n_TMB Note number=1 1: On edge of spectrum 2: Bad base line a: CH_3_OCHO 225900 in wing HDO 225896. b: CH_3_OCHO 258476/82/99 blended with CH_3_OCHO 261433/6 and CH_3_OCHO 258490/496/502/508/518/523. c: CH_3_OCHO 260384/392/404/415 thoroughly blended with CH_3_CN 257507/22/27 and CH_3_OCH_3_ 260400/1/3/5. d: CH_3_OCHO 261148 blended with CH_3_OCH_3_ 261145/47/48/50. e: CH_3_OCHO 334851 blended with CH_3_OH 337546. f: CH_3_OCHO 334877 blended with CH_3_OH 337519. g: CH_3_OCHO 338338 and CH_3_OCHO 338355 in wings CH_3_OH 338344. h: CH_3_OCHO 338396 and CH_3_OCHO 338414 in wings CH_3_OH 338404/408. i: CH_3_OCHO 343435/43 blended with CH_3_OH 340141. j: On wing OCS 28--27. k: CH_3_OCHO 344322/36/47 blended with SO 344310 and H^13^CO^+^ 4--3. l: CH_3_OCHO 344539 blended with HCS^+^ 8--7. m: CH_3_OCHO 345090 in wing H_2_CS 348531. n: CH_3_OCHO 358591 in wing CH_3_OH 358605. --- DV {DELTA}V km/s W Integrated intensity K.km/s n_W Note number=1 1: On edge of spectrum 2: Bad base line a: CH_3_OCHO 225900 in wing HDO 225896. b: CH_3_OCHO 258476/82/99 blended with CH_3_OCHO 261433/6 and CH_3_OCHO 258490/496/502/508/518/523. c: CH_3_OCHO 260384/392/404/415 thoroughly blended with CH_3_CN 257507/22/27 and CH_3_OCH_3_ 260400/1/3/5. d: CH_3_OCHO 261148 blended with CH_3_OCH_3_ 261145/47/48/50. e: CH_3_OCHO 334851 blended with CH_3_OH 337546. f: CH_3_OCHO 334877 blended with CH_3_OH 337519. g: CH_3_OCHO 338338 and CH_3_OCHO 338355 in wings CH_3_OH 338344. h: CH_3_OCHO 338396 and CH_3_OCHO 338414 in wings CH_3_OH 338404/408. i: CH_3_OCHO 343435/43 blended with CH_3_OH 340141. j: On wing OCS 28--27. k: CH_3_OCHO 344322/36/47 blended with SO 344310 and H^13^CO^+^ 4--3. l: CH_3_OCHO 344539 blended with HCS^+^ 8--7. m: CH_3_OCHO 345090 in wing H_2_CS 348531. n: CH_3_OCHO 358591 in wing CH_3_OH 358605. --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Jul 30 Frank Helmich <fph@deuterium.strw.LeidenUniv.nl> J_A+AS_124_205.xml Radial velocities. VIII. Ground based measurements for HIPPARCOS. J/A+AS/124/255 J/A+AS/124/255 Radial velocities measurements Radial velocities. VIII. Ground based measurements for HIPPARCOS. C Fehrenbach M Duflot C Mannone R Burnage V Genty Astron. Astrophys. Suppl. Ser. 124 255 1997 1997A&AS..124..255F J/A+AS/110/177 : Radial velocities measurements. VII. (Duflot+, 1995) III/190 : WEB Catalog of Radial Velocities (Duflot+ 1995) Fehrenbach C. et al., Paper I. =1987A&AS...71..263F Fehrenbach C. et al., Paper II. =1987A&AS...71..275F Fehrenbach C. et al., Paper III. =1990A&AS...83...91F Duflot M. et al., Paper IV =1990A&AS...83..251D Duflot M. et al., Paper V. =1992A&AS...94..479D Fehrenbach C. et al., Paper VI. =1992A&AS...95..541F Radial velocities catalogs Galaxy: kinematics and dynamics techniques: radial velocities We publish 1879 radial velocities of stars distributed in 105 fields of 4x4degres. We continue the PPO series (Fehrenbach et al. 1987A&AS...71..263F, 1987A&AS...71..275F, 1990A&AS...83...91F and 1992A&AS...95..541F; Duflot et al. 1990A&AS...83..251D, 1992A&AS...94..479D, 1992A&AS...95..541F and 1995A&AS..110..177D), using the Fehrenbach objective prism method.
Radial velocities HD HD number --- BD BD number --- SpType Spectral type --- No Number of the comparison star --- Vmag Visual magnitude mag Pmag Photographic magnitude mag RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin RV Radial velocity km/s e_RV rms uncertainty on RV km/s o_RV Number of measurements --- Bin *: visual binary --- r_RV2 Reference for radial velocity RV2 number=1 W : catalogue Wilson (1953), Cat. <III/21> E : catalogue Evans (1967), Cat. <III/47>) WEB: catalogue Wilson, Evans, Batten (1995), Cat. <III/190> B : catalogue Barbier (1989) Cat. <III/161> BP : bibliographie Barbier-Petit (1986A&AS...65...59B) COR: Coravel, private communication MAR: Marly, private communication MOY: mean radial velocity estimated by us, for several sources ORB: spectroscopic double stars catalogue from Batten (1989), Cat. <V/64> STN: Standard star for radial velocity # : the radial velocity is known, but has not been used for the field adjusting --- RV2 Radial velocity from litterature km/s e_RV2 rms uncertainty on RV2 km/s o_RV2 Number of measurements --- Field Field number PPO --- Individual radial velocities HD/BD HD or BD number --- JD Julian date of observation d RV Radial velocity km/s Field Field number PPO --- Patricia Bauer CDS 1996 Dec 05 M. Duflot <duflot@OBMARA.CNRS-MRS.FR> J_A+AS_124_255.xml The Westerbork Northern Sky Survey (WENSS). I. A 570 square degree Mini-Survey around the North Ecliptic Pole J/A+AS/124/259 J/A+AS/124/259 Westerbork Northern Sky Survey I. The Westerbork Northern Sky Survey (WENSS). I. A 570 square degree Mini-Survey around the North Ecliptic Pole R B Rengelink Y Tang A G de Bruyn G K Miley M N Bremer H J A Rottgering M A R Bremer Astron. Astrophys. Suppl. Ser. 124 259 1997 1997A&AS..124..259R Radio sources radio continuum: general surveys The Westerbork Nortern Sky Survey (WENSS) is a low-frequency (325 MHz) radio survey that will cover the whole sky north of a declination of 30 degrees A first installment of the survey covers an area of 570 square degrees around the North Ecliptic Pole. A source list comprising 11,299 sources and 994 components is listed in Table 6 of the paper. This table is presented here.
Catalogue of the Westerbork Northern Sky Survey (WENSS) sources in the NEP Mini-Survey. WENSS Name (IAU-format) --- m_WENSS Multiplicity index on WENSS number=1 Uppercase letters designate components. Lowercase letters were added in May 1999 to remove the name collisions. These concern 118 WNB names assigned to 237 sources. --- RAh Right Ascencion (B1950) h RAm Right Ascencion (B1950) min RAs Right Ascencion (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Type Single/Mult./Comp./Ext. Type number=2 S = Single component source M = Multiple component source C = Individual component E = extended source --- Flag Flag (*=Possible problem) --- Sp Peak flux density (in mJy/beam) mJy SI Integrated flux density (mJy) mJy MajAxis Major axis number=3 If the source is unresolved then a value of 0 is assigned to these parameters arcsec MinAxis Minor axis number=3 If the source is unresolved then a value of 0 is assigned to these parameters arcsec PA Position angle number=3 If the source is unresolved then a value of 0 is assigned to these parameters deg NSE Local noise level (in mJy/beam) mJy Frm Frame --- R.B. Rengelink Leiden Observatory 1996 Nov 22 Roeland Rengelink <wenss@strw.LeidenUniv.nl> UNKNOWN UNKNOWN * 22-Nov-1996: Prepared by R.B. Rengelink (Leiden Observatory) * 14-May-1999: Lowercase letters a, b or c were added in column m_WENSS to 118 WNB names (see "Note (1)" section above) J_A+AS_124_259.xml The variable light curve of BH Virginis J/A+AS/124/281 J/A+AS/124/281 BH Vir BV light curves The variable light curve of BH Virginis F Y Xiang Q Y Liu Astron. Astrophys. Suppl. Ser. 124 281 1997 1997A&AS..124..281X Binaries, spectroscopic Magnitudes binaries: eclipsing stars: individual (BH Vir) Photoelectric observations of the short period eclipsing binary BH Vir in B and V bands are presented. Comparing with earlier published observations, we found that there were smaller variations in the light curve (outside eclipse) in 1991 than in the previous data.
BH Vir HD 121909 13 58 24.8 -01 39 38 BD-01 2897 HD 122575 14 02 51.7 -02 22 32
Photoelectric measurements of BH Vir in B band Photoelectric measurements of BH Vir in V band HJD Heliocentric Julian date d mag(V-C) BV Vir minus BD-01 2897 magnitude Bmag for table1, Vmag for table2 mag Patricia Bauer CDS 1997 Mar 20 Yulan Yang <bily@public.km.yn.cn> J_A+AS_124_281.xml Spectroscopic and photometric study of the bright X-ray cluster A1300 J/A+AS/124/283 J/A+AS/124/283 BR magnitude and redshift of A1300 Spectroscopic and photometric study of the bright X-ray cluster A1300 M Pierre J Oukbir D Dubreuil G Soucail J -L Sauvageot Y Mellier Astron. Astrophys. Suppl. Ser. 124 283 1997 1997A&AS..124..283P Clusters, galaxy Magnitudes Redshifts galaxies: clusters: individual (Abell 1300) galaxies: distances and redshifts X-rays: galaxies We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15<=z<=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.
ACO 1300 11 32.0 -19 54
Photometric analysis of A1300 xpos x distance from the field center (cD) number=1 1 pix = 0.314" pix ypos y distance from the field center (cD) number=1 1 pix = 0.314" pix Rmag R magnitude (average between 2 frames) mag B-R B-R colour index (average between 4 frames) mag Rmorph Morphological class in the R band (see text) --- Spectroscopic analysis of A1300 No Internal number referring to Fig.7, 8 --- n_No Note on No number=1 *: Presence of emission lines: 101: H_{alpha} 103: H_{alpha} 115: [OII] at 3727, H_{beta}, [OIII] at 4959 and 5007, OI at 6300 and 6364, H_{alpha}, NII at 6549 and 6583, SII at 6717 and 6734 205: H_{alpha}, H_{beta}? 225: OI at 6300 and 6364 320: H_{alpha}? 321: H_{alpha}? SII at 6717 n: The two nuclei of the cD galaxy correspond to numbers 121 & 219 and show totally similar redshifts at the present spectroscopic resolution. --- RAdeg Right ascension (J2000) number=2 Galaxy positions were interactively measured on the STScI digitized blue sky survey images having a pixel size of 1.7", and should have an accuracy of ~3.4" deg DEdeg Declination (J2000) number=2 Galaxy positions were interactively measured on the STScI digitized blue sky survey images having a pixel size of 1.7", and should have an accuracy of ~3.4" deg z Redshift --- e_z Error on the redshift --- q_z z measurement quality number=3 1: highest peak in the correlation function, 2: 2nd peak, 9: interactive measurement with lines --- Rmag R magnitude (only for galaxies within the area processed for photometry) mag B-R B-R colour index mag Member Cluster member galaxy (3sigma clipping method) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Jan 24 Marguerite Pierre <mpierre@discovery.saclay.cea.fr> J_A+AS_124_283.xml The FUOR characteristics of the PMS star BN Orionis inferred from new spectroscopic and photometric observations J/A+AS/124/33 J/A+AS/124/33 BN Ori UBV photometry & equivalent width The FUOR characteristics of the PMS star BN Orionis inferred from new spectroscopic and photometric observations V S Shevchenko O Ezhkova H R E Tjin A Djie M E van den Ancker P F C Blondel D de Winter Astron. Astrophys. Suppl. Ser. 124 33 1997 1997A&AS..124...33S Equivalent widths Photometry, UBV Stars, pre-main sequence circumstellar matter stars: emission-line, Be stars: individual (BN Ori) stars: pre-main sequence BN Ori is a young emission-line star with a peculiar light curve. During the first half of this century the star showed strong irregular brightness-variations, similar to those of Herbig Ae stars. In the current half of the century the light curve resembles that of a FU Ori-object (FUOR, after Ambartsumian 1971Afz.....7..557A). It can be characterised by an initial large-scale rise in brightness followed by a gradual decay over a period of about 15-years. From various photometric patrol programmes we concluded that the star remained at the same brightness level for the last 30-years. Between 1991 and 1995 the spectrum of BN Ori was intensively observed and was found to exhibit some unique peculiarities. We have analysed the visual spectra obtained with the 6m BTA telescope of the SAO, the 60cm and 48cm telescopes at Mt. Maidanak, the 1.4m CAT and the 1.5m telescope of ESO and the UV-spectra obtained with the IUE in 1984 and 1986. The spectra show certain similarities with those of classical FUORs, such as a large-scale thermal stratification, with Balmer lines showing A6-A7 spectral type wings, while other lines are typical for late F-type stars. However, in contrast to classical FUORs, BN Ori is not of high luminosity-class. On the other hand the spectrum also shows similarities with those of Herbig A7e stars, although these stars have much stronger absorption lines in the UV from their outer shell and their circumstellar dust excesses are much larger than for BN Ori. Also, the rotation rate vsinii of BN Ori is between 180 and 220km/s, which is typical for A-type stars of 2-5M_{sun}_. This may indicate that BN Ori is a fast rotating FUOR with an intermediate-mass precursor on which the outburst had a different effect than in the case of the classical FUORs (which are rotating slower and have a low-mass T Tauri star as precursor). In the BN Ori outburst most of the massive gas- and dust shell, characteristic for Herbig Ae stars, seems to have been removed, except for the H{alpha}- and MgII-emission region close to the photosphere. The disappearance of the circumstellar dust shell may explain the drastic variability-change in the light curve of BN Ori. The mass-accretion rates of BN Ori and several Herbig A7e stars (derived from the analysis of their UV-spectra in terms of disc-accretion) suggest that the FUOR outburst in BN Ori was due to a thermal runaway (Bell, 1994ApJ...427..987B) in its inner accretion-disc which was triggered by a modest increase in the accretion rate.
BN Ori HD 245465 05 36 29.4 +06 50 01 HR 5999 HD 144668 16 08 34.2 -39 06 17 FU Ori 05 45 22.5 +09 04 12
Identification and source of lines in the high-resolution visual spectra of BN Ori, HR 5999 and FU Ori. lambda Wavelength 0.1nm Ident Line identification --- Ex Excitation energy eV S Line source number=1 p: photospheric c: chromospheric i: interstellar s: shell, c.s. envelope d: disc --- EW1 BN Ori equivalent width 0.1nm u_EW1 Uncertainty flag on EW1 --- n_EW1 Note on EW1 number=2 b: blended vs: very strong st: strong m: medium w: weak vw: very weak EW1 data are from BTO-spectrum Nov.21, 1991 data except when n_EW1=2 where data are from Kolotilov & Zajtseva (1976Afz....12...31K) EW2 data are from Tjin A Djie et al. (1989A&AS...78....1T) EW3 data are from Herbig (1966VA......8..109H) --- FW1 BN ORI Full width at half maximum km/s u_FW1 Uncertainty flag on FW1 --- EW2 HR 5999 equivalent width 0.1nm u_EW2 Uncertainty flag on EW2 --- n_EW2 Note on EW2 number=2 b: blended vs: very strong st: strong m: medium w: weak vw: very weak EW1 data are from BTO-spectrum Nov.21, 1991 data except when n_EW1=2 where data are from Kolotilov & Zajtseva (1976Afz....12...31K) EW2 data are from Tjin A Djie et al. (1989A&AS...78....1T) EW3 data are from Herbig (1966VA......8..109H) --- FW2 HR 5999 Full width at half maximum km/s n_FW2 + when two values of FW2, : uncertainty flag --- FW2b Second FWHM value when n_FW2="+" km/s EW3 FU Ori equivalent width 0.1nm n_EW3 Note on FU Ori equivalent width number=2 b: blended vs: very strong st: strong m: medium w: weak vw: very weak EW1 data are from BTO-spectrum Nov.21, 1991 data except when n_EW1=2 where data are from Kolotilov & Zajtseva (1976Afz....12...31K) EW2 data are from Tjin A Djie et al. (1989A&AS...78....1T) EW3 data are from Herbig (1966VA......8..109H) --- UBVR photometric data of BN Ori HJD Heliocentric Julian date d Vmag V magnitude mag U-B U-B colour index mag B-V B-V colour index mag V-R V-R colour index mag Tel Telescope number=1 1: Zeiss 600 reflector (60cm) 3: AZT 14 reflector (48cm) --- Obs Observer number=2 C: A.V. Chernyshev G: K.N. Grankin I: M.A. Ibragimov M: S.Yu Melnikov P: D.L. Portnov S: V.S. Shevchenko Y: S.D. Yakubov --- n_Obs Note on observations number=3 Simultaneous with the high-resolution spectrum from SAO (Sect.4.3) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Nov 12 P.F.C. Blondel <blondel@sara.nl> J_A+AS_124_33.xml UBV absolute CCD photometry and differential astrometry of close visual double stars, with G-type primaries. J/A+AS/124/353 J/A+AS/124/353 CCD UBV photometry of close visual doubles UBV absolute CCD photometry and differential astrometry of close visual double stars, with G-type primaries. T Nakos D Sinachopoulos E van Dessel Astron. Astrophys. Suppl. Ser. 124 353 1997 1997A&AS..124..353N Photometry, CCD Photometry, UBV Stars, double and multiple binaries: visual catalogs We present V magnitudes, (B-V) and (U-B) colours of close visual double star components, and their differences as well as separations and position angles of 40 visual double stars. The common properties of the members of this sample are the small angular separation {rho}, which is less than 7", and the common spectral type of the primaries, which are of G-type. The observations made with the Bessel U, B and V filters, while the astrometry was performed in the V filter only. For the observations, the CCD camera attached to the Cassegrain focus of the 90 cm Dutch telescope, at La Silla, Chile, had been used. From the analysis of the data we concluded that from the sample of the fourty double stars observed seven proved to be physical pairs, while the rest must have common origin components.
Astrometric results No Visual binary number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DM Durchmusterung designation of the primary --- rho Angular separation arcsec e_rho rms uncertainty on rho number=1 The very small values of e_rho are due to the assumption of {sigma}_r_({rho})=0. We took {sigma}_r_({rho})=0 for the error of the angular separation rho due to the atmospheric refraction. Realistic values of e_rho are probably one order of magnitude higher arcsec Theta Position angle deg e_Theta rms uncertainty on Theta deg Obs Epoch of observation yr Photometric results No Visual binary number --- DM DM number --- m_DM Multiplicity index on DM --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag U-B U-B colour index mag e_U-B rms uncertainty on U-B mag Photometric differences and angular separation of the components No Visual binary number --- DM DM or ADS number --- rho Angular separation arcsec DVmag Difference in V magnitude mag D(B-V) Difference in B-V colour index mag D(U-B) Difference in U-B colour index mag tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Dec 03 Dimitris Sinachopoulos <Dimitris.Sinachopoulos@oma.be> J_A+AS_124_353.xml The Ca II triplet lines as diagnostics of luminosity, metallicity and chromospheric activity in cool stars J/A+AS/124/359 J/A+AS/124/359 Ca II triplet lines in cool stars The Ca II triplet lines as diagnostics of luminosity, metallicity and chromospheric activity in cool stars S V Mallik Astron. Astrophys. Suppl. Ser. 124 359 1997 1997A&AS..124..359M Equivalent widths Spectroscopy Stars, atmospheres Stars, late-type galaxies: stellar content stars: chromospeheres stars: late-type CCD spectra of the infrared triplet lines of ionized calcium at {lambda}{lambda}8498, 8542, 8662 have been obtained at a spectral resolution of 0.4{AA} in 146 stars brighter than V=+7.0 spanning a range in spectral types from F7 to M4 of all luminosity classes and a range in metallicity [Fe/H] from -3.0 to +1.1. These have been analysed to investigate the dependence of the Ca II triplet strengths on stellar parameters like luminosity, temperature and metallicity. A detailed study reveals a strong dependence on luminosity, much stronger for metal rich stars than for the metal poor ones and a milder dependence on metallicity, although much more conspicuous in supergiants than in dwarfs. All these correlations are found to be non-linear over the parameter space covered. The present study also shows chromospheric activity to be an important phenomenon affecting the strength and the shape of the line profiles. Stars of similar luminosity and metallicity have varying Ca II line depths owing to varying chromospheric emission filling in their Ca II absorption. The Ca II triplet strength is thus observed to be a triparametric discriminant in cool stars.
Stellar parameters HD HD number, Cat. <III/135> --- HR HR number, Cat. <V/50> --- Name Star name --- Vmag V magnitude mag SpType Spectral type --- Teff Effective temperature K R-I R-I color index mag logg Gravity surface [cm/s2] n_logg Note on logg number=1 * denotes the stars for which log g was estimated from their stellar data using the procedure described in the text of the paper on p.6 --- [Fe/H] Metallicity [Sun] Measured line strengths of the Ca II triplet HD HD number, Cat. <III/135> --- HR HR number, Cat. <V/50> --- Name Star name --- EW8498 Equivalent width at lambda8498 0.1nm EW8542 Equivalent width at lambda8542 0.1nm EW8662 Equivalent width at lambda8662 0.1nm EWall Sum of EWs of all the three lines 0.1nm EW8542+EW8662 Sum of EWs of lambda8542 and lambda8662 0.1nm tables.tex TeX version of the tables Patricia Bauer CDS 1996 Nov 22 Sushma Mallik <sgvmlk@iiap.ernet.in> J_A+AS_124_359.xml Studies of dense molecular cores in regions of massive star formation. V. Structure and kinematics of dense cores from ammonia observations J/A+AS/124/385 J/A+AS/124/385 Dense molecular cores. V. Studies of dense molecular cores in regions of massive star formation. V. Structure and kinematics of dense cores from ammonia observations I Zinchenko T Henning K Schreyer Astron. Astrophys. Suppl. Ser. 124 385 1997 1997A&AS..124..385Z J/A+A/288/601 : Dense molecular cores. I. (Zinchenko+ 1994) J/A+AS/118/191 : Dense molecular cores. IV. (Juvela, 1996) Zinchenko I. et al., Paper I =1994A&A...288..601Z Zinchenko I. et al., Paper II =1995A&AS..111...95Z Zinchenko I., Paper III =1995A&A...303..554Z Juvela M., Paper IV =1996A&AS..118..191J Masers Radial velocities Radio lines ISM: clouds ISM: molecules radio lines: ISM stars: formation We present results of the observations of 17 molecular clouds associated with bright FIR sources in the NH_3_ (1, 1) and (2, 2) lines with the 100-m radio telescope in Effelsberg. The lines were detected in 11 clouds and 10 of them have been mapped in these lines. The kinetic temperatures, sizes, masses and mean densities of the ammonia cores have been derived. For most of the detected clouds the masses derived under the assumption of a relative ammonia abundance of {chi}(NH_3_)=3x10^-8^ are close to virial masses. However, in S 88 B the ratio M/M_vir_ is only ~0.1 and in a few other cases this ratio is significantly lower than unity which may indicate ammonia underabundance. Almost all objects with the signs of underabundance are among the most luminous IR sources in our sample. Most of the mapped cores are elongated with noticeable velocity gradients along the major axis. The most prominent example is S 255. S 87 has a two-component structure with 2 distinct velocity components which overlap partly spatially. In about half of the mapped sources the NH_3_ line widths increase near the peaks of the ammonia emission. The kinetic temperatures are centrally peaked. They reach 20-28K in the centre and drop to 15-20K at the edges of the ammonia emitting regions. In S 76 E a weak extended emission in the (1, 1) line at the velocity blue-shifted by ~5km/s relative to the core emission was detected. Hyperfine intensity anomalies in the (1, 1) transition were found in S 199 in addition to the known case of these anomalies in S 87.
Source list Name Source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg RG Galacto-centric distance of the source kpc Dist Distance from the Earth kpc r_Dist Distance reference number=1 a: Brand & Blitz (1993, Cat. <J/A+A/275/67>)) b: Plume et al. (1992ApJS...78..505P) c: Blitz et al. (1982ApJS...49..183B, Cat. <VII/50>) d: Henning et al. (1992A&AS...93..525H) e: Avedisova & Palous (1989BAICz..40...42A) f: Yang et al. (1991ApJ...373..137Y) g: Fich & Blitz (1984ApJ...279..125F) i: assumed --- z Height above the Galactic plane pc IRAS IRAS PSC (Cat. <II/125>) name --- n_IRAS Multiplicity index on IRAS --- L(IR) IRAS luminosity solLum Detec Source detection number=2 h: Outflow detected as given by Mattila et al. (1996, in prep.) o: Outflow detected as given by Wu et al. (1976, Cat. <J/A+AS/115/283>) --- Rem Remark --- NH3 mapping data for S76E NH3 mapping data for S86 NH3 mapping data for S87 NH3 mapping data for S88B NH3 mapping data for S145 NH3 mapping data for S199 NH3 mapping data for S231 NH3 mapping data for S255 NH3 mapping data for RNO1B NH3 mapping data for BFS48 Dalpha Offset in R.A. (multiplied by cos{delta}) arcsec Ddelta Offset in Dec. arcsec N Velocity component --- Vlsr LSR velocity km/s e_Vlsr rms uncertainty on Vlsr km/s DeltaV Line width km/s e_DeltaV rms uncertainty on DeltaV km/s l_logNH3 limit flag on logNH3 --- logNH3 Ammonia NH_3(1,1) column density cm-2 e_logNH3 rms uncertainty on logNH3 cm-2 Tkin Kinetic temperature K e_Tkin rms uncertainty on Tkin K Patricia Bauer CDS 1996 Dec 03 Igor Zinchenko <igor@gstar.Helsinki.FI> J_A+AS_124_385.xml Astrometric positions of stars with high proper motions in the Southern Hemisphere J/A+AS/124/437 J/A+AS/124/437 Southern high proper motion stars positions Astrometric positions of stars with high proper motions in the Southern Hemisphere J M Rousseau J P Perie Astron. Astrophys. Suppl. Ser. 124 437 1997 1997A&AS..124..437R I/230 : Southern Hemisphere Catalogue of Bordeaux (Rousseau+ 1996) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) Rousseau J.M., Perie J.P., Gachard M.T., 1995, Hemisphere Sud Catalogue de Bordeaux, Observatoire de Bordeaux, Vols. 1-5 Rousseau J.M., Perie J.P., Gachard M.T., 1996A&AS..116..301R, Cat. <I/230> Rousseau J.M., Perie J.P., 1996A&AS..115..517R Positional data Proper motions astrometry stars: kinematics Several stars with large proper motions, cited by W.J. Luyten, were included in the preliminary programme for the HIPPARCOS mission. When performing preparatory measurements of plates, difficulties were encountered in identifying certain of these stars when relying only on published coordinates. We have taken advantage of this work which relates to the southern sky in order to determine the astrometric position of the greatest possible number of these objects, even for those which were not included in the programme.
Catalogue LHS LHS number (Cat. <I/87>) --- m_LHS (1) --- r_mag Source of magnitude number=2 Various sources of magnitude are : "b" = Bessel's list (1990A&AS...83..357B) "r" = Rodgers and Eggen's list (1974PASP...86..742R) " " = Others (CDS, HIC, LHS Catalogue 1979) --- mag Magnitude (see n_mag) --- n_mag Filter of magnitude --- RAh Right ascension (J2000) at Epoch number=3 Positions for the equinox J2000 on the system FK4, at Epoch h RAm Right ascension (J2000) at Epoch number=3 Positions for the equinox J2000 on the system FK4, at Epoch min RAs Right ascension (J2000) at Epoch number=3 Positions for the equinox J2000 on the system FK4, at Epoch s DE- Declination sign --- DEd Declination (J2000) at Epoch number=3 Positions for the equinox J2000 on the system FK4, at Epoch deg DEm Declination (J2000) at Epoch number=3 Positions for the equinox J2000 on the system FK4, at Epoch arcmin DEs Declination (J2000) at Epoch number=3 Positions for the equinox J2000 on the system FK4, at Epoch arcsec pmRA Proper motion in right ascension (x cos(DE)) number=4 The cos(DE) factor is included in pmRAs Various sources are : - Positions and proper Motions (Roser & Bastian 1992, Cat. <I/193>) - Hipparcos Input Catalogue (Cat. <I/196>) - Luyten Half Second Catalogue (Cat. <I/87>) arcsec/yr pmDE Proper motion in declination number=4 The cos(DE) factor is included in pmRAs Various sources are : - Positions and proper Motions (Roser & Bastian 1992, Cat. <I/193>) - Hipparcos Input Catalogue (Cat. <I/196>) - Luyten Half Second Catalogue (Cat. <I/87>) arcsec/yr e_RA Deviation in right ascension (x cos(DE)) arcsec e_DE Deviation in declination arcsec Epoch-1900 Mean epoch of observation (-1900) yr Nmeas Number of measurements --- Note *: individual note number=5 Individual notes 10: Close double with LHS 9. Sep = 2.1". The pair is also V* UV Cet 29: Kapteyn's star 49: Proxima. Is also HIC 70890 110/111: Sep = 9" 118: Close double, sep = 0.7" (ADS 520). Is also LFT 55, CD-25 225 and HIC 2941 171/172: IDS 03160-6253, sep = 309" 222: Close double, sep = 2" (IDS 06549-4409). Is also HIC 33499 and Ci 20 407 289/290: Sep = 6.4" 308/309: Sep = 16.4" 386/387: ADS 9446, sep = 22.5" 415/416: Sep = 7" 437/438: IDS 17092-2627, sep = 5.4". Is also HIC 84405, GJ 663 520: Close double, sep = 0.1" (IDS 22160-7244) 1077/1078: Sep = 51" 1097/1098: IDS 00288-3532, sep = 5.2" 1110: Close double, sep = 0.1" (IDS 00324-3750). Is also HIC 2944 and LTT 330 1208: Close double : Rodgers A.W. and Eggen O.J. (1974PASP...86..742R) 1337/1338: IDS 02008-2833, sep = 58" 1409: Close double, sep = 0.5" (IDS 02243-2026). Is also HIC 11565, LFT 213 and GJ 100 1466/1467: IDS 02500-3618, sep = 36.7" 1515: Close double (ADS 2402). Is also LFT 261, CD-29 1177, Ci 20 211, HIC 14879 and GJ 127 1551/1552: IDS 03276-6317, sep = 54" 1724/1727: IDS 05004-5614, sep = 79" 1770/1771: IDS 05354-4609, HIC 26501, sep = 5" 1804: IDS 05566-3103AB, sep = 0.8". Is also HIC 28442, GJ 225.2 1911: Close double, sep = 0.6" (IDS 07146-4649). Is also LFT 521, HIC 35296 and GJ 269 1959/1960: IDS 07559-6002, sep = 61" 2253/2254: IDS 10188-5939, HIC 50808, sep = 9.4" 2296/2297: Sep = 16" 2379/2380: IDS 11104-1734, sep = 18.5" 2456/2457: IDS 11422-6512, sep = 16.3" 2647: Close double, sep = 1.9" (IDS 12479-1758). Is also LTT 4924 and HIC 62882 2806/2807: IDS 13432-3512, sep = 11.8" 2815: Possibly close double. Is also LFT 1044, CPD-56 5970, Ci 20 815 3427: Very large disagreement between proper motions PPM of Luyten (Cat. <I/87>) and Catalog of proper-motion stars III (Eggen 1987AJ.....93..379E) : (-0.585 -0.245) or permutation between mu_alpha, mu_delta 3635: Close double (IDS 20588-7334). Is also HIC 104440, GJ 818.1 3707: Close double (IDS 21395-5808). Is also LFT 1657, CPD-58 7893 and HIC 107522 3750/3751: Sep = 10.3" 3790: Close double, sep = 2" (IDS 22117-5406). Is also LFT 1702, HIC 110109 and GJ 853A 3921/3922: IDS 23110-6727, sep = 70" 4013: Is also CD-42 16457, LTT 9698, LFT 1823, V* SX Phe (Mv : 6.8/7.5) 5139a: Close double, sep = 1.9" (ADS 6914). Is also BD-22 2345, Ci 20 480, HIC 42430 5299a: Is also IDS 15410-3736A, CD-37 10500A, Ci 20 946, GJ 599A and HIC 77358 5299b: Is also IDS 15410-3736B, GJ 599B. LHS 5299a/5299b, sep = 15" 5399: Close double, sep = 1.4" (IDS 23107-4506). Is also HIC 114885 and CD-45 14980 --- Names Other identifiers --- Patricia Bauer CDS 1997 Jan 21 Ernst Paunzen <PAUNZEN@astro.ast.univie.ac.at> J_A+AS_124_437.xml B[e] stars. IV. HD 45677 = MWC 142 J/A+AS/124/441 J/A+AS/124/441 Spectroscopy of HD 45677 = MWC 142 B[e] stars. IV. HD 45677 = MWC 142 Y Andrillat C Jaschek M Jaschek Astron. Astrophys. Suppl. Ser. 124 441 1997 1997A&AS..124..441A J/A+AS/117/281 : B[e] stars. I. HD 51585 (= OY Gem) J/A+AS/118/495 : B[e] stars. II. MWC 349 A J/A+AS/120/99 : B[e] stars. III. MWC 645 Equivalent widths Spectra, infrared Spectroscopy stars: emission-line, Be stars: individual (HD 45677) stars: variables: other On the basis of spectroscopic CCD material obtained at the Haute Provence Observatory, we provide line identifications and equivalent width measurements in the wavelength regions 3750-5112 and 7065-10212{AA} of the spectrum of HD 45677. Over 235 features are identified and a comparison of our results with those of other authors is provided. We also discuss the variability of the lines using equivalent widths and the line spectrum. We conclude that the gaseous shell surrounding the star has a temperature of the order of 7000K and that its distance to the star is less than ten stellar radii. We discuss the similarity of this star to other stars previously analyzed.
HD 45677 MWC 142 06 28 17.4 -13 03 10
Unified list of lines measured in HD 45677 Lambda Laboratory wavelength 0.1nm n_Lambda Note on Lambda number=1 a = absorption characteristic of the line e = emission characteristic of the line ed = double emission * indicates that these lines come from a spectrum taken in 1990, whereas the rest of the Paschen series comes from a spectrum taken in 1993 Please notice that the regions 7000-7412 and 9025-9400 are very perturbed by atmospheric absorption. Wavelengths of unidentified lines are rounded off to the nearest tenth of Angstroem. --- EW Equivalent width 0.1nm n_EW Note on EW number=2 +p : refers to the preceding line +f : refers to the following line --- Ident Identification number=3 J: Johansson (1978PhS....18..217J) *: Nussbaumer and Storey (1982A&A...110..295N) Meinel: Meinel A.B., Aveni A.F. and Stockton M.W., 1969 Catalog of emission-lines in astrophysical objects, Tucson Vreux: Vreux et al. (1990A&A...238..207V) eta Car: Johansson (1977MNRAS.178p..17J) TV: Thackeray and Velasco (1976Obs....96..104T) --- Patricia Bauer CDS 1997 Jan 17 J_A+AS_124_441.xml Search for young low-mass stars in a ROSAT selected sample south of the Taurus-Auriga molecular clouds J/A+AS/124/449 J/A+AS/124/449 Young stars south of Taurus-Auriga Search for young low-mass stars in a ROSAT selected sample south of the Taurus-Auriga molecular clouds A Magazzu E L Martin M F Sterzik R Neuhaeuser E Covino J M Alcala Astron. Astrophys. Suppl. Ser. 124 449 1997 1997A&AS..124..449M Magnitudes Stars, pre-main sequence X-ray sources stars: formation stars: late-type stars: pre-main sequence X-rays: stars We present results of intermediate resolution spectroscopy of 131 optical counterparts to 115 ROSAT All-Sky Survey X-ray sources south of the Taurus-Auriga dark cloud complex. These objects have been selected as candidate young stars from a total of 1084 ROSAT sources in a ~300 square degree area. We identify 30 objects as low-mass PMS stars on the basis of the LiI{lambda}6708{AA} doublet in their spectrum, a signature of their young age. All these stars have a spectral type later than F7 and show spectral characteristics typical of weak-line and post-T Tauri stars. The presence of young objects several parsecs away from the regions of ongoing star formation is discussed in the light of the current models of T Tauri dispersal.
X-ray data for our sample ROSAT ROSAT (Cat. <IX/11>) name --- Counts Number of counts in the broad ROSAT band --- e_Counts rms uncertainty on Counts --- Exp Exposure time s HR1 Hardness ratio 1 --- e_HR1 rms uncertainty on HR1 --- HR2 Hardness ratio 2 --- e_HR2 rms uncertainty on HR2 --- ML Maximum likelihood of existence --- kTx Emission energy (typical error +/-0.55keV) keV log(NH) Absorbing foreground column density (typical error +/-0.77, in log(N_H_) cm^-2^) cm-2 FX X-ray flux (typical error +/-1.87.10^+13^mW/m2) 10+13mW/m2 Closest optical counterparts. ROSAT ROSAT name --- m_ROSAT Multiplicity index on ROSAT name --- RAh Optical right ascension (J2000.0) number=1 From the GSC (or Simbad if available) h RAm Optical right ascension (J2000.0) number=1 From the GSC (or Simbad if available) min RAs Optical right ascension (J2000.0) number=1 From the GSC (or Simbad if available) s DE- Declination sign --- DEd Optical declination (J2000.0) number=1 From the GSC (or Simbad if available) deg DEm Optical declination (J2000.0) number=1 From the GSC (or Simbad if available) arcmin DEs Optical declination (J2000.0) number=1 From the GSC (or Simbad if available) arcsec oRA Offset between X-ray and optical right ascension arcsec oDE Offset between X-ray and optical declination arcsec Vmag V magnitude (from the GSC <II/143> or Simbad if n_Vmag=:) mag n_Vmag : indicates that V magnitude is from Simbad --- log(FX/FV) X-ray to optical flux ratio --- Prob Discrimination probability --- Rem Remarks number=2 Some GSC counterparts appear on several GSC plates which may have different colors and different filters; we have always chosen the closest counterpart, i.e. we neither try to average the magnitudes nor indicate the plate color as GSC magnitudes are very uncertain anyway (about half a magnitude) 1: Not listed in the GSC 2: HD 23793 B (F5V) and the early-type star HR 1174 (B3) are an optical pair with 9" separation (Lindroos 1986A&A...156..223L); the later type star is more likely to be the true optical counterpart of the X-ray source (e.g. Schmitt et al. 1993ApJ...402L..13S) 3: Companion N is an unresolved binary itself 4: Not listed in the GSC. --- Other optical counterparts observed. ROSAT ROSAT name --- m_ROSAT Multiplicity index on ROSAT name --- RAh Optical right ascension (J2000.0) h RAm Optical right ascension (J2000.0) min RAs Optical right ascension (J2000.0) s DE- Declination sign --- DEd Optical declination (J2000.0) deg DEm Optical declination (J2000.0) arcmin DEs Optical declination (J2000.0) arcsec Pos Relative position to the counterpart listed in Table 2 --- Vmag V magnitude (from the GCS) mag Rem Remarks number=1 Remarks are either GSC, Simbad, or visual inspection of plates --- Results of spectroscopy of all counterparts ROSAT ROSAT name --- m_ROSAT Multiplicity index on ROSAT name --- Tel Telescope used number=1 Telescope used to observe the star: INT for the Isaac Newton Telescope ESO for the ESO1.52m telescope --- EW(Halpha) H{alpha} equivalent width (negative when in emission) 0.1nm n_EW(Halpha) Note on EW(Halpha) number=2 f: indicates that H{alpha} emission is filling in the absorption line a: for absorption without available equivalent width --- EW(Li) Lithium 6708A absorption equivalent width 0.1nm n_EW(Li) Note on EW(Li) number=3 ':': indicates large uncertainty n: no y: yes --- SpType Spectral type (always luminosity class V unless otherwise noted) --- Nature Nature of object (see text) --- Rem Remarks number=4 1: Spectrum blue-shifted by 2A 2: Star A itself is SB, with the secondary having almost the same spectral type as the primary 3: Also observed at INT 4: Spectrum blue-shifted by 1A, the H{alpha} line shows a P Cyg profile 5: H{alpha} line shows an inverse P Cyg profile 6: Spectrum red-shifted by 2A 7: SB: the primary is F8 with H{alpha} in absorption and W_{lambda}_(Ca)<W_{lambda}_(Li)=0.16A, the secondary has W_{lambda}_(Ca)>W_{lambda}_(Li)=0.13A, thus the system may by a close PMS binary; H{alpha} line shows a P Cyg profile 8: Very noisy spectrum 9: Secondary seems to have a slightly earlier spectral type. --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Dec 17 Antonio Magazzu <antonio@sunct.ct.astro.it> J_A+AS_124_449.xml The ATCA/VLA OH 1612 MHz survey. II. Observations of the Galactic Disk Region J/A+AS/124/509 J/A+AS/124/509 ATCA/VLA OH 1612 MHz survey. II. The ATCA/VLA OH 1612 MHz survey. II. Observations of the Galactic Disk Region M N Sevenster J M Chapman H J Habing N E B Killeen M Lindqvist Astron. Astrophys. Suppl. Ser. 124 509 1997 1997A&AS..124..509S J/A+AS/122/79 : Galactic Bulge Region OH 1612MHz survey I. (Sevenster+ 1997) Masers Radio lines Galaxy: stellar content radio lines: stars stars: AGB and post-AGB surveys We present observations of the region between -45{deg}<=l<=-10{deg} and |b|<=3{deg} in the OH 1612.231MHz line, taken in 1994 January with the Australia Telescope Compact Array (ATCA). These observations are part of a larger survey, covering |l|<=45{deg} and |b|<=3{deg}, with the ATCA and the Very Large Array. In a previous article we have discussed the observational strategy in detail. In this paper we present only the objects found in this part of the survey. The region was systematically searched for OH-maser emission and was covered completely with 910 pointing centres separated by 30'. We found 202 OH-masing objects, 112 of which are new detections. Out of the 202 objects, 166 have a standard double-peaked spectral profile, 32 a single-peaked profile and 4 objects have non-standard or irregular profiles. In this article we analyse the data statistically and give classifications and identifications with known sources where possible. The astrophysical, kinematical, morphological and dynamical properties of subsets of the data will be addressed in future articles.
Compact OH-maser sources No Source number --- Name Source name (based on galactic coordinates) --- Type Spectrum type --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Delta Position scatter arcsec R Offset from pointing centre arcmin VL Velocity blue-shifted peak km/s VH Velocity red-shifted peak km/s VC Velocity central star km/s VE Outflow velocity shell km/s SL Flux density blue-shifted peak Jy SH Flux density red-shifted peak Jy Rms Rms noise in empty cubes mJy Ref Number reference for previous detection number=1 1: te Lintel Hekkert P. et al., 1989A+AS....78..399T 2: Braz A. and Epchtein N., 1983A+AS....54..167B 3: Bowers P.F. and Knapp G.R., 1989ApJ.. 347..325B 4: te Lintel Hekkert P. et al. (1991), Cat. <J/A+AS/90/327> --- IRAS IRAS name of nearest IRAS point source --- Dist Distance to nearest IRAS PS as fraction of IRAS error ellipse --- fig6a.ps The spectra for all the sources in Table 1 fig6b.ps figure 6 continued fig6c.ps figure 6 continued fig6d.ps figure 6 continued fig6e.ps figure 6 continued fig6f.ps figure 6 continued fig6g.ps figure 6 continued fig6h.ps figure 6 continued table1.tex LaTeX version of table1 Sevenster Sterrewacht Leiden, NL Patricia Bauer CDS 1996 Dec 06 Maartje Sevenster <sevenste@strw.LeidenUniv.nl> J_A+AS_124_509.xml Revised photometric distances to nearby dwarf galaxies in the IC 342/Maffei complex J/A+AS/124/559 J/A+AS/124/559 VI photometry of dwarf galaxies Revised photometric distances to nearby dwarf galaxies in the IC 342/Maffei complex I Karanchentsev I Drozdovsky S Kajsin L O Takalo P Heinamaki M Valtonen Astron. Astrophys. Suppl. Ser. 124 559 1997 1997A&AS..124..559K Galaxies, photometry galaxies: distances and redshifts galaxies: irregular galaxies: stellar content Tables show the photometry and colour index for the observed galaxy, with the image parameter SHARP. This parameter is a measure of the difference between the observed width of the object and the psf model.
UGCA 105 05 14.3 +62 34 UGCA 92 04 32.0 +63 36 UGCA 86 03 59.8 +67 08 NGC 1569 04 30.7 +64 51 Cas 1 ZOAG 129.57+07.11 02 06.1 +69 01
Photometry of the stars in the galaxy UGCA 105 Photometry of the stars in the galaxy UGCA 92 Photometry of the stars in the galaxy UGCA 86 Photometry of the stars in the galaxy NGC 1569 Photometry of the stars in the galaxy Cas 1 No Star number ----- Xpos X coordinate number=1 The XY positions were calculated from the SW corner (X,Y=0,0) of the image, with +X going to east and +Y to north. This corner is the lower-right corner of the image. pix Ypos Y coordinate number=1 The XY positions were calculated from the SW corner (X,Y=0,0) of the image, with +X going to east and +Y to north. This corner is the lower-right corner of the image. pix Vmag V magnitude mag V-I V-I colour index mag V-R V-R colour index mag SHARP Image parameter SHARP number=2 SHARP is a measure of the difference between the observed width of the object and the width of the psf model. ---- L [01] Marks the stars inside the visible boundary of the galaxy ----- fig6.ps Galaxy UGCA 86 fig7.ps UGCA 86 V--V-I diagram fig8a.ps NGC 1569 Southern part fig8b.ps NGC 1569 Northern part fig9.ps NGC 1569 V--V-I diagram Patricia Bauer CDS 1997 Jan 06 Leo Takalo <TAKALO@sara.cc.utu.fi> J_A+AS_124_559.xml Southern and equatorial irregular variables. I. Photoelectric photometry J/A+AS/124/55 J/A+AS/124/55 Photometry of irregular variables Southern and equatorial irregular variables. I. Photoelectric photometry D Cieslinski F J Jablonski J E Steiner Astron. Astrophys. Suppl. Ser. 124 55 1997 1997A&AS..124...55C II/139 : General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988) II/140 : New Catalogue of Suspected Variable Stars (Kukarkin+, 1982) Booth L., Charles P.A., 1982, MNRAS 201, 25p =1982MNRAS.201p..25B Downes R.A., Shara M.M., 1993, PASP 105, 127 =1993PASP..105..127D Gregorio-Hetem J., Lepine J.R.D., Quast G.R., Torres C.A.O., de la Reza R., 1992, AJ 103, 549 =1992AJ....103..549G Kholopov P.N., et al., 1987, General Catalogue of Variable Stars-GCVS4, Nauka Publishing House, Moscow Ninger-Kosibowa S., 1955, Prace Wrocl. Tow. Naukowego Ser. B, Nr. 57 Torres C.A.O., Quast G.R., de la Reza R., Gregorio-Hetem J., Lepine J.R.D., 1995, AJ 109, 2146 =1995AJ....109.2146T Vogt N., Bateson F.M., 1982, A&AS 48, 383 =1982A&AS...48..383V Photometry, Cousins Photometry, UBVRI Stars, variable stars: AGB and post-AGB stars: variables: general surveys We present the results of an optical photometric survey of 616 irregular variables. The targets were selected among objects classified as L, L:, I, I:, IS and IS: in the General Catalogue of Variable Stars and New Catalogue of Suspected Variable Stars.
UBV(RI) photometry Name Star name --- HJD Heliocentric Julian day d Vmag V magnitude mag U-B U-B colour index mag B-V B-V colour index mag V-Rc V-R_c_ colour index mag Rc-Ic R_c_-I_c_ colour index mag e_Vmag Uncertainty on V magnitude mag e_U-B Uncertainty on U-B colour index mag e_B-V Uncertainty on B-V colour index mag e_V-Rc Uncertainty on V-R_c_ colour index mag e_Rc-Ic Uncertainty on R_c_-I_c_ colour index mag Rem See note number=1 *: Nights without calibration sequences (see discussion in the paper) 1: Averaged values of magnitude and colours. Object is a Mira variable 2: Averaged values of magnitude and colours. Object is a cataclysmic variable 3: 10 arcsec optical pair. Possible contamination 4: Classified as probable Herbig Ae/Be object in Gregorio-Hetem et al. (1992AJ....103..549G) 5: 10 arcsec optical pair (~2mag weaker) included in the diaphragm 6: Averaged values of magnitude and colours. Object is a symbiotic u star 7: Suggested as Cepheid variable by Booth & Charles (1982MNRAS.201p..25B) 8: Object is a RV Tauri variable 9: Optical pair (~2mag weaker) included in the diaphragm 10: Quoted as suspected of cataclysmic variable in Vogt & Bateson (1982A&AS...48..383V) and Downes & Shara (1993, Cat. <V/79>) 11: Quoted as suspected of cataclysmic variable of Z Cam type in the GCVS4 (kholopov et al. 1987, Cat. <II/139>) 12: Classified as T Tauri star in Torres et al. (1995AJ....109.2146T) 13: Carbon star 14: Optical pair. The two stars were included in the diaphragm 15: 5 arcsec optical pair (~3mag weaker) included in the diaphragm 16: Constant star. Possibly indicated wrongly in the finding chart of Ninger-Kosibowa (1955, Prace Wrocl. Tow. Naukowego Ser. B, Nr. 57) 17: 10 arcsec optical pair. The two stars were included in the diaphragm 18: 10 arcsec optical pair. Possible contamination 19: Object is a RR Lyrae variable 20: <10 arcsec optical pair. The two objects were included in the diaphragm 21: Optical pair. The two stars included in the diaphragm 22: Object is a Be star 23: 5 arcsec optical pair included in the diaphragm -------------------------------------------------------------------------------- Acknowledgements: Deonisio Cieslinski <deo@das.inpe.br> --- Patricia Bauer CDS 1996 Dec 09 J_A+AS_124_55.xml A survey of the stellar rotation in barred galaxies J/A+AS/124/61 J/A+AS/124/61 Stellar Rotation in SB0s A survey of the stellar rotation in barred galaxies D Bettoni G Galletta Astron. Astrophys. Suppl. Ser. 124 61 1997 1997A&AS..124...61B Radial velocities Velocity dispersion galaxies: elliptical and lenticular, cD galaxies: kinematics and dynamics We present stellar velocity- and velocity dispersion- data for 13 SB0 galaxies and one SBa, based on 61 spectra collected at ESO. We want to provide a database for the study of the stellar velocity and velocity dispersion fields and for future modeling. In the Table radii are in arcsec, velocity and velocity dispersion are in Km/s
NGC 3271 10 30.4 -35 21 NGC 4371 12 24.9 +11 42 NGC 4596 12 39.9 +10 11 NGC 4754 12 52.3 +11 19 NGC 6744 19 09.7 -63 51 NGC 7079 21 32.6 -44 04
Kinematical data for the sample galaxies Name Galaxy name --- PA Position angle of the spectrograph slit deg Oslit Offset of the slit with respect to the nucleus --- ExpTime Exposure time min Rad Radius arcsec HRV Heliocentric radial velocity km/s e_HRV rms uncertainty on HRV km/s sigma Velocity dispersion km/s e_sigma rms uncertainty on sigma km/s table5.tex LaTeX version of table5 Patricia Bauer CDS 1996 Oct 31 Daniela Bettoni <dbettoni@leda.pd.astro.it> J_A+AS_124_61.xml MSC - a catalogue of physical multiple stars J/A+AS/124/75 J/A+AS/124/75 Multiple star catalogue MSC - a catalogue of physical multiple stars A A Tokovinin Astron. Astrophys. Suppl. Ser. 124 75 1997 1997A&AS..124...75T Positional data Radial velocities Stars, double and multiple binaries: general catalogs Data on 728 stellar systems of multiplicity 3 to 7 are given. All systems are physical and, with little exception, hierarchical. They are represented as several "elementary binaries". For each binary the orbital period and separation are given, as well as component magnitudes, spectral types and estimated masses. Orbital elements are also given when available. The present (1999) version of the catalogue is updated as compared to the original 1997 publication, with some changes in the format.
Catalogue of Physical Multiple Stars (systems) IDS IDS (based on 1900 position) --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec pmRA Proper motion in RA mas/yr pmDE Proper motion in DE mas/yr RV Radial velocity km/s plx Parallax arcsec r_plx Parallax code number=1 Parallax code: HIP - trigonometric Hipparcos p12 - spectroscopic for components 1,2 GL - trigonometric from Gliese catalogue DYN - dynamical from visual orbit ORB - orbital for visual/SB2 orbit bib - taken from literature --- nComp Number of Components (Multiplicity) --- TRAP T for trapezia --- Name Name --- Individual subsystems IDS IDS(1900) --- Level Level in hierarchy number=1 Level in hierarchy: 1 11 12 111 112 121 122 and so on... --- Comp Component designation --- Type Observing technique/status number=2 Discovery/observing status code: c - wide, possibly C.P.M. system C - C.P.M. system (sep.>3"); The following small letters give the criteria used: h - hypothetical parallax, r - radial velocities, p - photometric distances, m - proper motions. v - close visual or interferometric system (sep.<3") V - visual system with computed orbit a - astrometric system (perturbed motion suspected) A - astrometric orbit for invisible companion is computed s - possibly spectroscopic system (var. RV or composite sp.) S1, S2 - spectroscopic system with computed orbit, single- or double-lined o - occultation binary E - eclipsing binary with known period e - eclipsing binary, period not known --- logP Logarithm (10) of period in days d Sep Separation or axis --- x_Sep Units of sep. (',",m) --- PA Position angle deg Vmag1 V-magnitude of the primary mag SP1 Spectral type of the primary --- Vmag2 V-magnitude of the secondary mag SP2 Spectral type of the secondary --- Mass1 Mass of the primary solMass MCode1 Mass estimation code for primary number=3 Mass codes: * - given in the original publication a - estimated from spectral type or B-V color index from Allen tables s - sum of masses for the sub-system(s) q - estimated from primary mass and mass ratio of SB2 m - minimum secondary mass for SB1 v - estimated from magnitude difference of a visual binary : - uncertain, magnitude difference assumed to be 2 mag. --- Mass2 Mass of the secondary solMass MCode2 Mass estimation code for secondary number=3 Mass codes: * - given in the original publication a - estimated from spectral type or B-V color index from Allen tables s - sum of masses for the sub-system(s) q - estimated from primary mass and mass ratio of SB2 m - minimum secondary mass for SB1 v - estimated from magnitude difference of a visual binary : - uncertain, magnitude difference assumed to be 2 mag. --- Rem Remark --- Orbital parameters IDS IDS(1900) --- Level Level in hierarchy --- Period Period (see X_period for the units) --- x_Period Units of period (d,y) --- T Periastron epoch (y or JD-2400000) --- e Eccentricity --- a Semi-major axis (see x_a fir the units) --- x_a Units of axis (",m) --- Node P.A. of the node deg LongP Longitude of periastron deg n_Node 'A' if primary node, 'B' otherwise --- Incl Inclination deg K1 Primary semi-amplitude km/s K2 Secondary semi-amplitude km/s V0 Center of mass velocity km/s Comm Comment, reference --- Remarks IDS IDS(1900) --- Rem Remark text --- IDS-WDS-HD-BD-HIP-HR-ADS cross-index IDS IDS(1900) --- COMP Component designation (* for primary comp.) --- WDS WDS(2000) (Cat. <I/237>) --- HD HD (Cat. <III/135>) number --- DM BD (Cat. <I/122>), CD (Cat. <I/114>) or CPD (Cat. <I/108>) identifier --- HIP HIPPARCOS (Cat. <I/239>) number --- HR HR (Cat. <V/50>) number --- ADS ADS number --- Patricia Bauer CDS 1999 Jun 03 Andrei Tokovinin <toko@sai.msu.ru> UNKNOWN UNKNOWN * 21-May-1996: first installed at CDS * 04-Dec-1998: 2 errors detected and corrected in file "catalog" * 01-Jun-1999: updated version supplied by Andrei Tokovinin J_A+AS_124_75.xml Further search for OH emission from IRAS sources. J/A+AS/124/85 J/A+AS/124/85 OH emission from IRAS sources Further search for OH emission from IRAS sources. V I Slysh A M Dzura I E Val'tts E Gerard Astron. Astrophys. Suppl. Ser. 124 85 1997 1997A&AS..124...85S II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) Infrared sources Masers Radio lines ISM: clouds ISM: molecules masers radio lines: ISM surveys Results of a continued search for OH main line emission from IRAS sources are reported. Towards a sample of 182 sources which consists of IRAS sources selected by the colour criterion for ultracompact HII region, and several IRAS cores, H_2_O masers and bipolar outflows, we detected 19 new OH masers of Class I and 5 OH/IR candidates. The correlation between IR and OH maser flux is confirmed. Also 51 thermal and 4 absorption sources were detected. The low radial velocities and derived OH column densities suggest that the thermal OH emission comes from nearby dark clouds. There is evidence that IRAS sources towards which thermal emission was detected are connected with these dark clouds.
IRAS
Masers Name IRAS or other names --- n_Name Note number=1 a: 1665 V profile centered at -21km/s and 1665 H profile at -27km/s were not observed with high velocity resolution. b: Detection reported in the Paper I. --- GLON Galactic longitude deg GLAT Galactic latitude deg V(1667MHz) Velocity (Gaussian fit for 1667MHz line) km/s e_V(1667MHz) rms uncertainty on V(1667MHz) km/s FWHM(1667MHz) FWHM (Gaussian fit for 1667MHz line) km/s e_FWHM(1667MHz) rms uncertainty on FWHM(1667MHz) km/s l_S1667MHz Limit flag on S1667MHz --- S1667MHz Flux (Gaussian fit for 1667MHz line) Jy e_S1667MHz rms uncertainty on S1667MHz Jy Pol Polarization type number=2 R: right circular polarization L: left circular polarization H: horizontal linear polarization V: vertical linear polarization T: line supposed to be thermal --- V(1665MHz) Velocity (Gaussian fit for 1665MHz line) km/s e_V(1665MHz) rms uncertainty on V(1665MHz) km/s FWHM(1665MHz) FWHM (Gaussian fit for 1665MHz line) km/s e_FWHM(1665MHz) rms uncertainty on FWHM(1665MHz) km/s l_S1665MHz Limit flag on S1665MHz --- S1665MHz Flux (Gaussian fit for 1665MHz line) Jy e_S1665MHz rms uncertainty on S1665MHz Jy Pol2 Polarization type number=2 R: right circular polarization L: left circular polarization H: horizontal linear polarization V: vertical linear polarization T: line supposed to be thermal --- Note c: 1665Mhz parameters are 1612MHz OH line ones (For 17269-2235 only) --- OtherName Other name --- Thermal sources Name IRAS or other names --- Lynds Associations of an IRAS source with nebulae of Lynds --- GLON Galactic longitude deg GLAT Galactic latitude deg l_S1667MHz Limit flag on S1667MHz --- S1667MHz Flux at 1667MHz (result of Gaussian fits) Jy l_S1665MHz Limit flag on S1667MHz --- S1665MHz Flux at 1665MHz (result of Gaussian fits) Jy RV Radial velocity (result of Gaussian fits) km/s FWHM FWHM (result of Gaussian fits) km/s N(OH) Estimates of OH column density. 10+14cm-2 V(CO) CO radial velocities km/s r_V(CO) Reference for radial velocity number=1 1: Myers et al. (1983ApJ...264..517) 2: Terebey et al. (1989ApJ...340..472T) 3: Casoli et al. (1986A&A...169..281C) 4: Heyer et al. (1987ApJ...321..370H) 5: Wouterloot and Brand (1989, Cat. <J/A+AS/80/149>) 6: de Geus et al. (1990A&A...231..137D) 7: Benson et al. (1989) --- IRAScloud Name of a associated IRAS cloud or core (Wood et al. 1994, Cat. <J/ApJS/95/457>) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Nov 12 Eric Gerard <Eric.Gerard@obspm.fr> J_A+AS_124_85.xml CHIANTI - an atomic database for emission lines. I. Wavelengths greater than 50 Angstroms J/A+AS/125/149 J/A+AS/125/149 CHIANTI - An Atomic Database For Emission Lines I. CHIANTI - an atomic database for emission lines. I. Wavelengths greater than 50 Angstroms K P Dere E Landi H E Mason B C Monsignori Fossi P R Young Astron. Astrophys. Suppl. Ser. 125 149 1997 1997A&AS..125..149D Atomic physics astronomical data bases: miscellaneous atomic data stars: atmospheres Sun: atmosphere ultraviolet: general A comprehensive set of accurate atomic data is required for analyses of astrophysical and solar spectra. CHIANTI provides a database of atomic energy levels, wavelengths, radiative data and electron excitation data for ions which are abundant in cosmic plasmas. The most recent electron excitation data have been assessed and stored following the method of Burgess & Tully (1992A&A...254..436B). The current version is essentially complete for specifying the emission spectrum at wavelengths greater than 50{AA}. A list of observed lines in the spectral region between 50 and 1100{AA} has been compiled and compared with the lines predicted by the CHIANTI database. The CHIANTI database reproduces the vast majority of lines observed at these wavelengths. CHIANTI includes IDL (Interactive Data Language) routines to calculate optically thin synthetic spectra for equilibrium conditions. IDL routines to calculate theoretical line intensities required for electron density or temperature diagnostics and emission measure studies are also included. The CHIANTI atomic database and supporting IDL routines are available by anonymous FTP.
A list of observed lines and lines in the CHIANTI database between 50 and 1100 Angstroms LamObs Observed wavelength from literature sources number=1 The observed wavelength is given as 0. if there is not report of an observed line at the wavelength of a reasonably intense line predicted by CHIANTI 0.1nm LamCH Wavelength in CHIANTI database 0.1nm Ion Ion (spectroscopic notation) --- Level1 Description of lower level of transition --- --- Separation dash --- Level2 Description of upper level of transition --- Int Predicted intensity of line in a small solar flare number=2 The intensity is given a 0. if the line is identified but is not included in the CHIANTI database. mW/m2/sr Ref Literature sources of observed wavelength number=3 References: 1: Acton et al. (1985ApJ...291..865A) 2: Behring et al. (1972ApJ...175..493B) 3: Behring et al. (1976ApJ...203..521B) 4: Dere (1978ApJ...221.1062D) 5: Freeman & Jones (1970SPh....15..288F) 6: Thomas & Neupert (1994, Cat. <J/ApJS/91/461>) 7: Widing & Sandlin (1968ApJ...152..545W) 8: Kastner et al. (1974ApJ...191..261K) 9: Burton & Ridgeley (1970SPh....14....3B) 10: Feldman & Doschek (1991ApJS...75..925F) --- table3.tex LaTeX version of table3 Patricia Bauer CDS 1997 Apr 22 Ken Dere <dere@halcyon.nrl.navy.mil> J_A+AS_125_149.xml NTT CCD photometry of the globular cluster M 79 = NGC 1904 in UBV J/A+AS/125/1 J/A+AS/125/1 The globular cluster NGC 1904 NTT CCD photometry of the globular cluster M 79 = NGC 1904 in UBV V Kravtsov A Ipatov N Samus O Smirnov G Alcaino W Liller F Alvarado Astron. Astrophys. Suppl. Ser. 125 1 1997 1997A&AS..125....1K Clusters, globular Photometry, CCD globular clusters: individual (M 79) Hertzsprung-Russell (HR diagram) Table 2 contains CCD UBV photometry of 2451 stars in the globular cluster NGC 1904. In the printed version, only the first 30 lines of the table were presented for guidance.
NGC 1904 M 79 05 24.3 -24 31
CCD photometry in M 79 No Running number --- Xpos X coordinate number=1 X coordinate is along right ascension and increases from West to East, Y coordinate is along declination and increases from North to South. pix Ypos Y coordinate number=1 X coordinate is along right ascension and increases from West to East, Y coordinate is along declination and increases from North to South. pix Vmag V magnitude mag U-B =-999.000 U-B color index mag B-V B-V color index mag Patricia Bauer CDS 1996 Sep 19 Nikolai N. Samus <samus@sai.msu.su> J_A+AS_125_1.xml Elemental abundance analyses with Complejo Astronomico El Leoncito REOSC echelle spectrograms. II. {mu} Leporis, 7 Sextantis, HR 4817, and 28 Herculis J/A+AS/125/219 J/A+AS/125/219 Abundances of mu Lep, 7 Sex, HR 4817 & 28 Her Elemental abundance analyses with Complejo Astronomico El Leoncito REOSC echelle spectrograms. II. {mu} Leporis, 7 Sextantis, HR 4817, and 28 Herculis S J Adelman O I Pintado Astron. Astrophys. Suppl. Ser. 125 219 1997 1997A&AS..125..219A Abundances Stars, peculiar stars: abundances stars: chemically peculiar stars: individual (mu Lep, 28 Her, 7 Sex, HR 4817) Elemental abundances are derived for four sharp-lined stars, the Mercury-Manganese stars {mu} Lep, HR 4817, and 28 Her, and 7 Sex, a Population I star with Population II space motions, using REOSC echelle spectrograms obtained at CASLEO to extend previous studies. Comparisons with published equivalent widths indicate that the CASLEO scale is marginally larger than those of DAO Reticon and KPNO CCD spectra. The CASLEO spectrograms have improved the quality of the abundance determinations. New abundances are found for a few elements.
mu Leo HD 85503 09 52 46.6 +26 00 28 HD 85504 7 Sex 09 52 12.7 +02 27 10 HR 4817 HD 110073 12 39 52.6 -39 59 13 HD 149121 28 Her 16 32 35.6 +05 31 16
Atomic abundances (table3 to table6) Name Star name --- Ion Ion --- Nline Number of lines --- Element Element (identical to bytes 9-10) --- l_log(Nel/Ntot) Limit flag on log(Nel/Ntot) --- log(Nel/Ntot) Derived abundance of Element (ratio of number of atoms to the total number of atoms per unit volume) --- e_log(Nel/Ntot) rms uncertainty on log(Nel/Ntot) --- u_e_log(Nel/Ntot) Uncertainty flag on e_log(Nel/Ntot) --- New lines (table3 to table6) Name Star name --- Ion Ion --- Mult Multiplet number --- lambda Wavelength 0.1nm log(gf) log(gf) value --- r_log(gf) Reference for log(gf) number=1 HL : Hubeny I. et al., 1994, Daresbury Lab. New. Anal. Astron. Spectra, No.20, p. 30 KX : Kurucz, 1995, in Astrophysical Applications of Powerful New Databases, eds. S. J. Adelman and W. L. Wiese (ASP, San Francisco), ASP Conf. Ser. 78, 205 MF : Fuhr et al. 1988, J. Phys. Chem. Ref. Data 15, Suppl. 4 MW : Martin et al., 1988, J. Phys. Chem. Ref. Data 15, Suppl. 3 WF : Wiese et al., 1996, J. Phys. Chem. Ref. Data, Monograph 6 WS : Wiese et al., 1966, NSRDS-NBS 4, US Government Printing, Office, Washington, DC --- EW Equivalent width 10-4nm log(N/Ntot) Derived abundance in relative number of atoms --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Oct 17 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> J_A+AS_125_219.xml Redshift of clusters and galaxies towards the Shapley Concentration J/A+AS/125/247 J/A+AS/125/247 Shapley Concentration galaxies velocities Redshift of clusters and galaxies towards the Shapley Concentration H Quintana J Melnick D Proust L Infante Astron. Astrophys. Suppl. Ser. 125 247 1997 1997A&AS..125..247Q Clusters, galaxy Redshifts galaxies: clusters: general large-scale structure of universe We report velocity measurements of galaxies in this, the densest mass concentration within z=0.1, obtained with the multifiber spectrograph MEFOS at ESO, La Silla. We derive redshifts of a number of Abell clusters and draw implications for the supercluster structure. The clusters A3554, A3566, A3577 and AS718 are confirmed as members, while the clusters A3524, A3531, A3542, A3545 and A3549 are shown to be background systems and A3581 a foreground one
Galaxy velocities and comparison with literature in the Cluster A 1060 Arm Arm sequential number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Rmag Visual R magnitude mag MType Morphological type --- HVel Heliocentric velocity km/s e_HVel rms uncertainty on HVel km/s RMag Absolute R magnitude mag HVelr Heliocentric velocity from literature km/s e_HVelr rms uncertainty on HVelr km/s Galaxy velocities in Abell Clusters in the Shapley Supercluster Region Abell Cluster name --- Arm Arm number in the cluster --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Rmag Visual R magnitude mag MType Morphological type --- n_MType Note on Mtype number=1 1: Lauberts & Valentijn, 1989, Cat. <VII/115> 2: Vettolani et al., 1990AJ.....99.1709V 3: Postman & Lauer, 1995ApJ...440...28P 4: Fairall & Jones, 1991, Cat. <VII/142> 5: Allen et al., 1991MNRAS.248..528A --- HVel Heliocentric velocity km/s e_HVel rms uncertainty on HVel km/s RMag Absolute R magnitude mag Com Comments number=1 1: Lauberts & Valentijn, 1989, Cat. <VII/115> 2: Vettolani et al., 1990AJ.....99.1709V 3: Postman & Lauer, 1995ApJ...440...28P 4: Fairall & Jones, 1991, Cat. <VII/142> 5: Allen et al., 1991MNRAS.248..528A --- Galaxy velocities from literature Abell Cluster name --- Gal Galaxy name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Rmag Visual R magnitude mag MType Morphological type --- HVel Heliocentric velocity km/s e_HVel rms uncertainty on HVel km/s ref References number=1 1: Allen et al., 1991MNRAS.248..528A 2: Mathews et al., 1995AJ....110..581M 3: Lauberts & Valentijn, 1989, Cat. <VII/115> 4: Vettolani et al., 1990AJ.....99.1709V 5: Postman & Lauer, 1995ApJ...440...28P 6: Quintana et al., 1995, Cat. <J/AJ/110/463> 7: Bade et al., 1995, Cat. <J/A+AS/110/469> 8: Strauss et al., 1992, Cat. <II/174> --- Patricia Bauer CDS 1997 May 23 J_A+AS_125_247.xml Radial velocities of planetary nebulae towards the Galactic bulge J/A+AS/125/289 J/A+AS/125/289 Planetary nebulae radial velocities Radial velocities of planetary nebulae towards the Galactic bulge A A Zijlstra A Acker J R Walsh Astron. Astrophys. Suppl. Ser. 125 289 1997 1997A&AS..125..289Z V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) J/ApJS/98/659 : Galactic PNe statistical distance scale (Zhang 1995) Planetary nebulae Radial velocities Galaxy: center Galaxy: kinematics and dynamics planetary nebulae: general stars: kinematics techniques: radial velocities The table lists the heliocentric radial velocities for planetary nebulae in the direction of the Galactic bulge. The accuracy is about 2km/s. The measurements were made in June and July 1993, using the ESO CAT with spectral resolution of 30000-60000. Halpha, [NII] 6548 and 6584 and [O III] 5007 were observed.
Radial velocities of bulge PN PNG PN ident (derived from l,b, see cat. <V/84>) --- Name Common name --- HRV Heliocentric velocity km/s n_HRV Note on Heliocentric velocity number=1 Velocities derived from: 1: [O III]; 2: H{alpha}, [NII]; 3: HeII --- Dist Adopted distance from the Sun kpc Patricia Bauer CDS 1997 Jan 10 Albert Zijlstra <azijlstr@eso.org> J_A+AS_125_289.xml Radial velocities and iron abundances of field RR Lyraes. I. J/A+AS/125/313 J/A+AS/125/313 RR Lyrae radial velocities and [Fe/H] I. Radial velocities and iron abundances of field RR Lyraes. I. J Fernley T G Barnes Astron. Astrophys. Suppl. Ser. 125 313 1997 1997A&AS..125..313F J/A+AS/125/321 : RR Lyrae radial velocities and [Fe/H] II. (Solano+ 1997) Abundances, [Fe/H] Radial velocities Stars, variable binaries: spectroscopic stars: abundances stars: individual (V363 Cas, AT And) stars: kinematics stars: variables: general We present systemic velocities and iron abundances for 56 RR Lyraes, the majority of which have been observed by the HIPPARCOS satellite. Comparison between our systemic velocities and previous values identifies several binary candidates only one of which, TU UMa, was previously suspected of being a binary. However, spectra of the unusual RR Lyrae BB Vir show no evidence of line doubling and hence do not support the recent claims that this star may have a Blue Horizontal Branch companion. Comparison between our abundances and previous determinations shows reasonable agreement except with the recent work of Layden (1994, Cat. <J/AJ/108/1016>) where we find systematic differences. Several of the stars included on the HIPPARCOS observing list as RR Lyraes are shown to be mis-classified. Of particular interest are the stars V363 Cas and AT And which, by analogy with XZ Cet, may be anomalous Cepheids.
Radial velocities and metal abundances of RR Lyr Name Star name --- RAh Right Ascension 2000 (hours) number=5 Position added to the original table (taken from SIMBAD) h RAm Right Ascension 2000 (minutes) number=5 Position added to the original table (taken from SIMBAD) min RAs Right Ascension 2000 (seconds) number=5 Position added to the original table (taken from SIMBAD) s DE- Declination 2000 (sign) number=5 Position added to the original table (taken from SIMBAD) --- DEd Declination 2000 (degrees) number=5 Position added to the original table (taken from SIMBAD) deg DEm Declination 2000 (minutes) number=5 Position added to the original table (taken from SIMBAD) arcmin Per Pulsation period d Note Note on star number=1 *: See Section 5 for a discussion of this star for which the classification as an RR Lyrae is uncertain &: only one observation of this star was made; hence the larger errors. Based on the large amplitude shown in the GCVS it is assumed to be an 'ab' type c: c-type, blank indicates ab-type --- [Fe/H] Abundance calculated in this work Sun [Fe/H]1 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]1 [1/9] Reference for [Fe/H]1 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> --- [Fe/H]2 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]2 [1/9] Reference for [Fe/H]2 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> --- [Fe/H]3 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]3 [1/9] Reference for [Fe/H]3 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> --- [Fe/H]4 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]4 [1/10] Reference for [Fe/H]4 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> --- [Fe/H]5 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]5 [1/10] Reference for [Fe/H]5 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> --- [Fe/H]6 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]6 [1/9] Reference for [Fe/H]6 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> --- Vsys Systemic velocity calculated in this work km/s e_Vsys rms uncertainty on Vsys km/s Vsys1 Systemic velocity taken from the literature km/s e_Vsys1 rms uncertainty on Vsys1 km/s r_Vsys1 [1/21] Reference for Vsys1 number=4 Sources of mean radial velocities: 1: Liu & Janes (1990ApJ...354..273L) 2: Jones et al. (1988ApJ...332..206J) 3: Hawley & Barnes (1985PASP...97..551H) 4: Woolley & Ali (1966RGOB..114....1W) 5: Farquhar (1948ApJ...107..276F) 6: Rogers (1960Obs....80..220R) 7: Varsavsky (1960ApJ...131..623V) 8: Cacciari et al. (1987A&AS...69..135C) 9: Burki & Meylan (1986A&A...156..131B) 10: Barnes et al. (1988ApJS...67..403B) 11: Layden (1994AJ....108.1016L), Cat <J/AJ/108/1016> 12: Imbert (1980A&A....86..259I) 13: Preston et al. (1961ApJ...133..484P) 14: Saha & White (1990PASP..102..148S) 15: Payne-Gaposhkin (1954AnHar.113....3P) 16: Woolley and Savage (1971RGOB..170....1W) 17: Joy (1938PASP...50..302J) 18: Joy (1950PASP...62...60J) 19: Joy (1955PASP...67..420J) 20: Preston (1959ApJ...130..507P) 21: Notni 1956, mitt. Jena No. 26 --- Vsys2 Systemic velocity taken from the literature km/s e_Vsys2 rms uncertainty on Vsys2 km/s r_Vsys2 [1/21] Reference for Vsys2 number=4 Sources of mean radial velocities: 1: Liu & Janes (1990ApJ...354..273L) 2: Jones et al. (1988ApJ...332..206J) 3: Hawley & Barnes (1985PASP...97..551H) 4: Woolley & Ali (1966RGOB..114....1W) 5: Farquhar (1948ApJ...107..276F) 6: Rogers (1960Obs....80..220R) 7: Varsavsky (1960ApJ...131..623V) 8: Cacciari et al. (1987A&AS...69..135C) 9: Burki & Meylan (1986A&A...156..131B) 10: Barnes et al. (1988ApJS...67..403B) 11: Layden (1994AJ....108.1016L), Cat <J/AJ/108/1016> 12: Imbert (1980A&A....86..259I) 13: Preston et al. (1961ApJ...133..484P) 14: Saha & White (1990PASP..102..148S) 15: Payne-Gaposhkin (1954AnHar.113....3P) 16: Woolley and Savage (1971RGOB..170....1W) 17: Joy (1938PASP...50..302J) 18: Joy (1950PASP...62...60J) 19: Joy (1955PASP...67..420J) 20: Preston (1959ApJ...130..507P) 21: Notni 1956, mitt. Jena No. 26 --- Vsys3 Systemic velocity taken from the literature km/s e_Vsys3 rms uncertainty on Vsys3 km/s r_Vsys3 [1/21] Reference for Vsys3 number=4 Sources of mean radial velocities: 1: Liu & Janes (1990ApJ...354..273L) 2: Jones et al. (1988ApJ...332..206J) 3: Hawley & Barnes (1985PASP...97..551H) 4: Woolley & Ali (1966RGOB..114....1W) 5: Farquhar (1948ApJ...107..276F) 6: Rogers (1960Obs....80..220R) 7: Varsavsky (1960ApJ...131..623V) 8: Cacciari et al. (1987A&AS...69..135C) 9: Burki & Meylan (1986A&A...156..131B) 10: Barnes et al. (1988ApJS...67..403B) 11: Layden (1994AJ....108.1016L), Cat <J/AJ/108/1016> 12: Imbert (1980A&A....86..259I) 13: Preston et al. (1961ApJ...133..484P) 14: Saha & White (1990PASP..102..148S) 15: Payne-Gaposhkin (1954AnHar.113....3P) 16: Woolley and Savage (1971RGOB..170....1W) 17: Joy (1938PASP...50..302J) 18: Joy (1950PASP...62...60J) 19: Joy (1955PASP...67..420J) 20: Preston (1959ApJ...130..507P) 21: Notni 1956, mitt. Jena No. 26 --- Vsys4 Systemic velocity taken from the literature km/s e_Vsys4 rms uncertainty on Vsys4 km/s r_Vsys4 [1/21] Reference for Vsys1 number=4 Sources of mean radial velocities: 1: Liu & Janes (1990ApJ...354..273L) 2: Jones et al. (1988ApJ...332..206J) 3: Hawley & Barnes (1985PASP...97..551H) 4: Woolley & Ali (1966RGOB..114....1W) 5: Farquhar (1948ApJ...107..276F) 6: Rogers (1960Obs....80..220R) 7: Varsavsky (1960ApJ...131..623V) 8: Cacciari et al. (1987A&AS...69..135C) 9: Burki & Meylan (1986A&A...156..131B) 10: Barnes et al. (1988ApJS...67..403B) 11: Layden (1994AJ....108.1016L), Cat <J/AJ/108/1016> 12: Imbert (1980A&A....86..259I) 13: Preston et al. (1961ApJ...133..484P) 14: Saha & White (1990PASP..102..148S) 15: Payne-Gaposhkin (1954AnHar.113....3P) 16: Woolley and Savage (1971RGOB..170....1W) 17: Joy (1938PASP...50..302J) 18: Joy (1950PASP...62...60J) 19: Joy (1955PASP...67..420J) 20: Preston (1959ApJ...130..507P) 21: Notni 1956, mitt. Jena No. 26 --- appen.tex LaTeX version of appen Patricia Bauer CDS 1997 Feb 18 Enrique Solano <ESM@v3500.vilspa.esa.es> J_A+AS_125_313.xml Radial velocities and iron abundances of field RR Lyraes. II. J/A+AS/125/321 J/A+AS/125/321 RR Lyrae radial velocities and [Fe/H] II. Radial velocities and iron abundances of field RR Lyraes. II. E Solano R Garrid J Fernley T G Barnes Astron. Astrophys. Suppl. Ser. 125 321 1997 1997A&AS..125..321S J/A+AS/125/313 : RR Lyrae radial velocities and [Fe/H] I. (Fernley+ 1997) Abundances, [Fe/H] Radial velocities Stars, variable stars: abundances stars: kinematics stars: variables: general This is the second of the papers devoted to derive radial velocities and iron abundances of field RR Lyraes observed by HIPPARCOS. Our abundances show good agreement with those in the literature obtained both from photometric ({DELTA}S index) and spectroscopic methods. Binary candidates and stars misclassified as RR Lyraes in the original HIPPARCOS list have been also identified.
Radial velocities and metal abundances of RR Lyr Name Star name --- RAh Right Ascension 2000 (hours) number=4 The position was added at CDS from SIMBAD data-base h RAm Right Ascension 2000 (minutes) number=4 The position was added at CDS from SIMBAD data-base min RAs Right Ascension 2000 (seconds) number=4 The position was added at CDS from SIMBAD data-base s DE- Declination 2000 (sign) number=4 The position was added at CDS from SIMBAD data-base --- DEd Declination 2000 (degrees) number=4 The position was added at CDS from SIMBAD data-base deg DEm Declination 2000 (minutes) number=4 The position was added at CDS from SIMBAD data-base arcmin Per Pulsation period d Type c: c-type, else ab-type --- Vsys Systemic velocity calculated in this work km/s e_Vsys rms uncertainty on Vsys km/s Vsys1 Systemic velocity taken from the literature km/s e_Vsys1 rms uncertainty on Vsys1 km/s r_Vsys1 [1/18] Reference for Vsys1 number=1 Sources of mean radial velocities: 1: Liu & Janes (1990ApJ...354..273L) 2: Jones et al. (1988ApJ...332..206J) 3: Hawley & Barnes (1985PASP...97..551H) 4: Woolley & Ali (1966RGOB..114....1W) 5: Varsavsky (1960ApJ...131..623V) 6: Cacciari et al. (1987A&AS...69..135C) 7: Burki & Meylan (1986A&A...156..131B) 8: Barnes et al. (1988ApJS...67..403B) 9: Layden (1994AJ....108.1016L), Cat <J/AJ/108/1016> 10: Imbert (1980A&A....86..259I) 11: Preston et al. (1961ApJ...133..484P) 12: Saha & White (1990PASP..102..148S) 13: Joy (1938PASP...50..302J) 14: Joy (1950PASP...62...60J) 15: Preston (1959ApJ...130..507P) 16: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 17: Clube et al. (1969MmRAS..72..101C) 18: Meylan et al. (1986A&AS...64...25M) --- Vsys2 Systemic velocity taken from the literature km/s e_Vsys2 rms uncertainty on Vsys2 km/s r_Vsys2 [1/18] Reference for Vsys2 number=1 Sources of mean radial velocities: 1: Liu & Janes (1990ApJ...354..273L) 2: Jones et al. (1988ApJ...332..206J) 3: Hawley & Barnes (1985PASP...97..551H) 4: Woolley & Ali (1966RGOB..114....1W) 5: Varsavsky (1960ApJ...131..623V) 6: Cacciari et al. (1987A&AS...69..135C) 7: Burki & Meylan (1986A&A...156..131B) 8: Barnes et al. (1988ApJS...67..403B) 9: Layden (1994AJ....108.1016L), Cat <J/AJ/108/1016> 10: Imbert (1980A&A....86..259I) 11: Preston et al. (1961ApJ...133..484P) 12: Saha & White (1990PASP..102..148S) 13: Joy (1938PASP...50..302J) 14: Joy (1950PASP...62...60J) 15: Preston (1959ApJ...130..507P) 16: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 17: Clube et al. (1969MmRAS..72..101C) 18: Meylan et al. (1986A&AS...64...25M) --- Vsys3 Systemic velocity taken from the literature km/s e_Vsys3 rms uncertainty on Vsys3 km/s r_Vsys3 [1/18] Reference for Vsys3 number=1 Sources of mean radial velocities: 1: Liu & Janes (1990ApJ...354..273L) 2: Jones et al. (1988ApJ...332..206J) 3: Hawley & Barnes (1985PASP...97..551H) 4: Woolley & Ali (1966RGOB..114....1W) 5: Varsavsky (1960ApJ...131..623V) 6: Cacciari et al. (1987A&AS...69..135C) 7: Burki & Meylan (1986A&A...156..131B) 8: Barnes et al. (1988ApJS...67..403B) 9: Layden (1994AJ....108.1016L), Cat <J/AJ/108/1016> 10: Imbert (1980A&A....86..259I) 11: Preston et al. (1961ApJ...133..484P) 12: Saha & White (1990PASP..102..148S) 13: Joy (1938PASP...50..302J) 14: Joy (1950PASP...62...60J) 15: Preston (1959ApJ...130..507P) 16: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 17: Clube et al. (1969MmRAS..72..101C) 18: Meylan et al. (1986A&AS...64...25M) --- Vsys4 Systemic velocity taken from the literature km/s e_Vsys4 rms uncertainty on Vsys4 km/s r_Vsys4 [1/18] Reference for Vsys1 number=1 Sources of mean radial velocities: 1: Liu & Janes (1990ApJ...354..273L) 2: Jones et al. (1988ApJ...332..206J) 3: Hawley & Barnes (1985PASP...97..551H) 4: Woolley & Ali (1966RGOB..114....1W) 5: Varsavsky (1960ApJ...131..623V) 6: Cacciari et al. (1987A&AS...69..135C) 7: Burki & Meylan (1986A&A...156..131B) 8: Barnes et al. (1988ApJS...67..403B) 9: Layden (1994AJ....108.1016L), Cat <J/AJ/108/1016> 10: Imbert (1980A&A....86..259I) 11: Preston et al. (1961ApJ...133..484P) 12: Saha & White (1990PASP..102..148S) 13: Joy (1938PASP...50..302J) 14: Joy (1950PASP...62...60J) 15: Preston (1959ApJ...130..507P) 16: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 17: Clube et al. (1969MmRAS..72..101C) 18: Meylan et al. (1986A&AS...64...25M) --- [Fe/H] Abundance calculated in this work Sun [Fe/H]1 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]1 [1/13] Reference for [Fe/H]1 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> 11: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 12: Clube et al. (1969MmRAS..72..101C) 13: Lub (1979AJ.....84..383L) --- [Fe/H]2 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]2 [1/13] Reference for [Fe/H]2 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> 11: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 12: Clube et al. (1969MmRAS..72..101C) 13: Lub (1979AJ.....84..383L) --- [Fe/H]3 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]3 [1/13] Reference for [Fe/H]3 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> 11: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 12: Clube et al. (1969MmRAS..72..101C) 13: Lub (1979AJ.....84..383L) --- [Fe/H]4 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]4 [1/13] Reference for [Fe/H]4 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> 11: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 12: Clube et al. (1969MmRAS..72..101C) 13: Lub (1979AJ.....84..383L) --- [Fe/H]5 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]5 [1/13] Reference for [Fe/H]5 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> 11: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 12: Clube et al. (1969MmRAS..72..101C) 13: Lub (1979AJ.....84..383L) --- [Fe/H]6 Abundance taken from the literature number=2 {DELTA}S values from previous work have been transformed to [Fe/H] using [Fe/H] = -0.13-0.195{DELTA}S (Fernley & Barnes 1996). As discussed in the text, the uncertainty in the [Fe/H] values, both from previous work and this work, is typically +/-0.13 dex. Sun r_[Fe/H]6 [1/13] Reference for [Fe/H]6 number=3 Sources of abundances: 1: Butler (1975ApJ...200...68B) 2: Kemper (1982AJ.....87.1395K) 3: Preston (1959ApJ...130..507P) 4: Clementini et al. (1991AJ....101.2168C) 5: Kinman & Caretta (1992PASP..104..111K) 6: Smith (1990PASP..102..124S) 7: Suntzeff et al. (1991ApJ...367..528S) 8: Layden (1994AJ....108.1016L), Cat. <J/AJ/108/1016> 9: Lambert et al. (1996ApJS..103..183L) 10: Clementini et al. (1995AJ....110.2319C), Cat. <J/AJ/110/2319> 11: Fernley & Barnes (1997A&AS..125..313F), Cat. <J/A+AS/125/313> 12: Clube et al. (1969MmRAS..72..101C) 13: Lub (1979AJ.....84..383L) --- appen.tex LaTeX version of appen Patricia Bauer CDS 1997 Feb 18 Enrique Solano <ESM@v3500.vilspa.esa.es> J_A+AS_125_321.xml Radial velocities and spectrophotometric properties of Southern Binary Galaxies J/A+AS/125/329 J/A+AS/125/329 Southern binary galaxies radial velocities Radial velocities and spectrophotometric properties of Southern Binary Galaxies R E de Souza D F de Mello S dos Anjos Astron. Astrophys. Suppl. Ser. 125 329 1997 1997A&AS..125..329D J/A+AS/110/371 : Southern binary galaxies. I. (Soares+, 1995) Galaxies, photometry Radial velocities galaxies: interactions galaxies: stellar content We present spectrophotometry of a sample of 26 Southern binary galaxies. 17 pairs were confirmed to be physically associated with typical separation of 136h^-1^kpc. Pairs with velocity difference {DELTA}V>=600km/s are probably not physically bound. A comparison with field galaxies suggests that galaxies in pairs tend to have a younger population probably stimulated by tidal interaction. No correlation between the young population and projected separation was found. This table contains the quantities derived from the spectral data.
Quantities derived from the spectral data Obj Identification of the pairs (Soares et al, 1995, Cat. <J/A+AS/110/371>) --- ESO ESO-LV (Cat. <VII/34>) identification number --- BT Blue Total magnitudes from ESO-LV mag MType Numerical code for morphological type --- RVabs Radial velocity from absorption lines km/s e_RVabs rms uncertainty on Vabs km/s q_RVabs Tonry and Davis (1979AJ.....84.1511T) quality parameter Note [P] P for peculiar morphological type number=1 Actually there is no quality parameter for n1741, since the spectra of this object is so rich in emission lines that the cross correlation technique could not be used. --- Max Peak value of correlation spectra --- RVems Radial velocity from emission lines km/s e_RVems rms uncertainty on Vems km/s Nlin Number of emission lines --- RVZcat Radial velocity from Zcat (Cat. <VII/193>) km/s R40 Blue Excess --- DRV Difference of radial velocity for the true pairs km/s Sep Separation of each pair arcsec Patricia Bauer CDS 1997 Feb 04 Ronaldo de Souza <ronaldo@kbrita.iagusp.usp.br> J_A+AS_125_329.xml New variable stars in the globular cluster NGC 288 J/A+AS/125/337 J/A+AS/125/337 New variables in NGC 288 New variable stars in the globular cluster NGC 288 J Kaluzny W Krzeminski M Nalezyty Astron. Astrophys. Suppl. Ser. 125 337 1997 1997A&AS..125..337K Clusters, globular Stars, variable binaries: close blue stragglers globular clusters: individual (NGC 288) stars: horizontal-branch stars: variables: other We report discovery of 3 new faint variables in the globular cluster NGC 288: 2 SX Phe stars and 1 contact binary. Both SX Phe variables are blue stragglers. The contact binary is located below cluster turnoff, slightly to the red of the main sequence. New photometry of 6 previously known variables is also presented. We note that 26 out of a total 43 SX Phe stars identified recently in {omega} Cen and NGC 288 exhibit V-band light curves with full amplitudes smaller than 0.10mag. The sample of known SX Phe stars is likely to be significantly incomplete in regard to the low amplitude variables.
NGC 288 V2 00 52 46.64 -26 34 07.4 NGC 288 V3 00 52 40.21 -26 32 28.8 NGC 288 V4 00 52 42.80 -26 34 45.4 NGC 288 V5 00 52 44.98 -26 33 52.1 NGC 288 V6 00 52 42.40 -26 34 54.6 NGC 288 V7 00 52 41.39 -26 33 59.7 NGC 288 V8 00 52 44.27 -26 33 59.6 NGC 288 V9 00 52 42.88 -26 34 09.6 NGC 288 V10 00 52 47.86 -26 33 01.9
V-band light curve of variable V2 V-band light curve of variable V3 V-band light curve of variable V4 V-band light curve of variable V5 V-band light curve of variable V6 V-band light curve of variable V7 V-band light curve of variable V8 V-band light curve of variable V9 V-band light curve of variable V10 HJD Heliocentric Julian date d Vmag V magnitude mag e_Vmag Error of V magnitude mag Janusz Kaluzny ? 1997 Nov 18 Janusz Kaluzny <jka@vela.astrouw.edu.pl> J_A+AS_125_337.xml A catalogue of the observations of the mutual phenomena of the Galilean satellites made in 1991 during the PHEMU91 Campaign J/A+AS/125/399 J/A+AS/125/399 Mutual phenomena of the Galilean satellites A catalogue of the observations of the mutual phenomena of the Galilean satellites made in 1991 during the PHEMU91 Campaign J -E Arlot C Ruatti W Thuillot J Arsenijevic R Baptista J Barroso Jr. C Bauer J Berthier C Blanco P Bouchet J Bourgeois H J J Bulder R Burchi J A Cano R Casas F Chauvet D Chis F Colas J Colin V D'Ambrosio G De Angelis G De Benedetto H Denzau J M Desbats P Descamps A Dipaolantonio A Dumitrescu L Farcas M Federspiel T Flatres M Froeschle O Gherega J M Gomez-Forrellad J Guarro O Hainaut A Horvat G Helmer D Hube Y Ito M Kidger J Lecacheux J F Le Campion J C Le Floch A Mallama B E Martin J F Mellilo C Meyer S Molau G Montignac B Morando B Nicolet B Nitschelm G Oprescu A Piersimoni D Przewozny V Protitch-Benishek M Rapaport A Riou J J Sacre F Sevre V Shkodrov J Souchay H Takami R Taylor D J Tholen V Turcu R Vasundhara J Vidal D T Vu G White R P Wilds Astron. Astrophys. Suppl. Ser. 125 399 1997 1997A&AS..125..399A Occultations Planets astrometry occultations planets and satellites: individual (Jupiter) planets and satellites: individual (satellites of Jupiter) In this paper, all the light-curves obtained during the PHEMU91 campaign of observations of the mutual phenomena of the Galilean satellites are presented. These observations give accurate astrometric positions of major interest for dynamical studies of the motion of the Galilean satellites. The aim of this work is to give observational data directly usable for theoretical studies. We made 374 observations of 111 mutual events from 56 sites. The accuracy of each observation has been deduced from a comparison with the theoretical predictions. For each observation, information is given about the telescope, the receptor, the site and the observational conditions. Other data as well as the data of the lightcurves themselves are available on the server: ftp://ftp.bdl.fr/pub/NSDC/jupiter/pheno_mut/1991
Observed mutual events Date Gregorian date of the phenomenon "DD/MM/YY" S1 First satellite involved --- Phe Type of phenomenon number=1 O: Occultation, E: Eclipse --- S2 Second satellite involved --- Type Type of phenomenon number=2 an: annular, pa: partial, pe: penumbra --- TB1h Predicted hour of the beginning of the event (UTC) with E-2 theory h TB1m Predicted minute of the beginning of the event (UTC) with E-2 theory min TB1s Predicted second of the beginning of the event (UTC) with E-2 theory s TM1h Predicted hour of the maximum of the event (UTC) with E-2 theory h TM1m Predicted minute of the maximum of the event (UTC) with E-2 theory min TM1s Predicted second of the maximum of the event (UTC) with E-2 theory s TE1h Predicted hour of the end of the event (UTC) with E-2 theory h TE1m Predicted minute of the end of the event (UTC) with E-2 theory min TE1s Predicted second of the end of the event (UTC) with E-2 theory s Mdrop1 Magnitude drop with E-2 theory mag TB2h Predicted hour of the beginning of the event (UTC) with E-3 theory h TB2m Predicted minute of the beginning of the event (UTC) with E-3 theory min TB2s Predicted second of the beginning of the event (UTC) with E-3 theory s TM2h Predicted hour of the maximum of the event (UTC) with E-3 theory h TM2m Predicted minute of the maximum of the event (UTC) with E-3 theory min TM2s Predicted second of the maximum of the event (UTC) with E-3 theory s TE2h Predicted hour of the end of the event (UTC) with E-3 theory h TE2m Predicted minute of the end of the event (UTC) with E-3 theory min TE2s Predicted second of the end of the event (UTC) with E-3 theory s Mdrop2 Magnitude drop with E-3 theory mag TB3h Predicted hour of the beginning of the event (UTC) with G-5 theory h TB3m Predicted minute of the beginning of the event (UTC) with G-5 theory min TB3s Predicted second of the beginning of the event (UTC) with G-5 theory s TM3h Predicted hour of the maximum of the event (UTC) with G-5 theory h TM3m Predicted minute of the maximum of the event (UTC) with G-5 theory min TM3s Predicted second of the maximum of the event (UTC) with G-5 theory s TE3h Predicted hour of the end of the event (UTC) with G-5 theory h TE3m Predicted minute of the end of the event (UTC) with G-5 theory min TE3s Predicted second of the end of the event (UTC) with G-5 theory s Mdrop3 Magnitude drop with G-5 theory mag TB4h Predicted hour of the beginning of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites h TB4m Predicted minute of the beginning of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites min TB4s Predicted second of the beginning of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites s TM4h Predicted hour of the maximum of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites s TM4m Predicted minute of the maximum of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites h TM4s Predicted second of the maximum of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites h TE4h Predicted hour of the end of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites min TE4m Predicted minute of the end of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites s TE4s Predicted second of the end of the event (UTC) with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites h Mdrop4 Magnitude drop with G-5 theory number=3 Predicted times with G-5 theory taking into account the scattering light from the surface of the satellites mag Dist Distance from the satellites to the center of Jupiter in Jovian radii. --- Site of observation of the mutual events Date Observation date "DD/MM/YY" Phen Phenomenon --- n_Phen Note when two phenomenons occur at the same date number=1 a: annular p: partial or penumbral b: Second event when the same event occurs at the same date --- Site Name of the site of observation --- TMINh Hour (UTC) of the minimum of light observed h TMINm Minute (UTC) of the minimum of light observed min TMINs Second (UTC) of the minimum of light observed s Lflux Lightflux drop in arbitrary units --- C-O Calculated minus Observed time computed with the G-5 prediction s Inst Code for the instrument used number=2 T for reflector, L for refractor (i.e. Lunette) --- Apert Aperture of the instrument in centimeters (for some instruments) cm Recept Code for the receptor --- EJup Elevation of Jupiter upon the horizon deg ESun Elevation of the Sun upon the horizon deg ObsCond Conditions of observation code number=3 1: Very good conditions 2: Acceptable conditions 3: Very difficult conditions --- Filter Code for the filter --- IntTime Time of integration s Size Size of the diaphragm or window (CCD) arcsec n_Size x when two lengths for a rectangular CCD window --- Size2 Second length for a rectangular CCD window arcsec Order Order number of satellites in diaphragm, i.e. the satellites, the global magnitude drop of which was observed --- e_TMINs Uncertainty on the observed time of the minimum of light s e_Lflux Uncertainty on the lightflux drop --- table2.tex LaTeX Version of table2 fig3_1.ps lightcurves observed from 13/11/90 to 05/01/91 fig3_2.ps lightcurves observed from 05/01/91 to 12/01/91 fig3_3.ps lightcurves observed from 12/01/91 to 19/01/91 fig3_4.ps lightcurves observed from 19/01/91 to 22/01/91 fig3_5.ps lightcurves observed from 22/01/91 to 29/01/91 fig3_6.ps lightcurves observed from 29/01/91 to 05/02/91 fig3_7.ps lightcurves observed from 05/02/9 to 13/02/91 fig3_8.ps lightcurves observed from 13/02/91 to 20/02/91 fig3_9.ps lightcurves observed from 20/02/91 to 02/03/91 fig3_10.ps lightcurves observed from 02/03/91 to 09/03/91 fig3_11.ps lightcurves observed from 09/03/91 to 16/03/91 fig3_12.ps lightcurves observed from 16/03/91 to 18/03/91 fig3_13.ps lightcurves observed from 18/03/91 to 01/04/91 fig3_14.ps lightcurves observed from 01/04/91 to 03/04/91 fig3_15.ps lightcurves observed from 05/04/91 to 10/04/91 fig3_16.ps lightcurves observed from 10/04/91 to 22/04/91 fig3_17.ps lightcurves observed from 22/04/91 to 29/04/91 fig3_18.ps lightcurves observed from 29/04/91 to 08/05/91 fig3_19.ps lightcurves observed from 10/05/91 to 07/06/91 fig3_20.ps lightcurves observed from 11/06/91 to 29/03/92 Arlot et al. BDL - URA707 Patricia Bauer CDS 1996 Dec 09 William Thuillot <William.Thuillot@bdl.fr> J_A+AS_125_399.xml UBV photometry and period variations of V839 Ophiuchi J/A+AS/125/407 J/A+AS/125/407 UBV photometry of V839 Ophiuchi UBV photometry and period variations of V839 Ophiuchi A Akalin E Derman Astron. Astrophys. Suppl. Ser. 125 407 1997 1997A&AS..125..407A Binaries, eclipsing Photometry, UBV binaries: eclipsing stars: individual (V839 Oph) A complete period variation analysis and new light curves of V839 Oph together with new ephemeris data are presented. The period variation was found to be dP/dt=3.1x10^-7d/yr. The period increament indicates that the conservative mass transfer rate from the less massive component to the more massive one is 6.5x10^-7M_sun_/yr. We fitted parabolic and we discuss the possible detection of sinusoidal curves to the (O-C) diagram and sinusoidal oscillations with period of about 20yr and semi-amplitude of 0.0065 day. A simultaneous solution of the B and V light curves was computed using the Wilson-Devinney synthetic light-curve code. The light curve solution indicates that the A-type W UMa-type system is in contact with a filling factor of ~39%.
V839 Oph HD 166231 (variable star) 18 09 21.3 +09 09 04 BD+09 3578 HD 166099 (comparison star) 18 08 50.6 +09 04 16 BD+08 3590 HD 166048 (check star) 18 08 33.6 +09 00 50
The data for light curves and colours of V839 Oph between 1989 and 1994 HJD Heliocentric Julian day d DVmag Diferential V magnitude number=1 Differential measurement in the sense variable minus comparison, after the correction for differential atmospheric extinction mag DBmag Diferential B magnitude number=1 Differential measurement in the sense variable minus comparison, after the correction for differential atmospheric extinction mag DUmag Diferential U magnitude number=1 Differential measurement in the sense variable minus comparison, after the correction for differential atmospheric extinction mag D(B-V) Diferential (B-V) colour mag D(U-B) Diferential (U-B) colour mag Epochs of minimum light of V839 Oph HJDMin Heliocentric Julian day at minimum light d Type Type of the minimum --- Data Data used to find the minimum number=1 v: visual pg: photographic pe: photoelectric --- Epoch Epoch number d (O-C) Linear ephemeris d (O-C)'q Residuals from the quadratic ephemeris d (O-Cs)' Residuals from the best fit d Ref Source of the minima time number=2 Sources : 1) Rigollet, 1947LAstr..61...54R 2) Binnendijk, 1960AJ.....65...79B 3) Wilaon and O'Toole, 1965PASP...77...58W 4) Diethelm, 1974BBSAG..16....1D 5) Diethelm, 1974BBSAG..17....1D 6) Diethelm, 1975BBSAG..23....1D 7) Diethelm, 1976BBSAG..29....1D 8) Braune et al., 1981AN....302...53B 9) Diethelm, 1978BBSAG..39....1D 10) Diethelm, 1979BBSAG..44....1D 11) Diethelm, 1981BBSAG..56....1D 12) This paper (data from Lafta and Grainger, 1985Ap&SS.114...23L) 13) Kreiner, 1988Roczn..59....1K 14) Ferrand, 1985BBSAG..58....1F 15) Niarchos, 1988IBVS.3156....1N 16) Kohl, 1985BBSAG..77....1K 17) Diethelm, 1985BBSAG..77....1D 18) Hanzl, 1990IBVS.3423....1H 19) this paper 20) Hanzl, 1991IBVS.3615....1H 21) Paschke, 1990BBSAG..96....1P 22) Blattler , 1991BBSAG..98....1B 23) Hanzl, 1994IBVS.4097....1H 24) Agerer and Hubscher, 1995IBVS.4222....1A 25) Demircan et al., 1994IBVS.4126....1D --- Ayvur Akalin Ankara University Observatory 1997 Dec 16 Ayvur Akalin-Peletier <Ayvur.Akalin-Peletier@durham.ac.uk> J_A+AS_125_407.xml Obscured AGB stars in the Magellanic Clouds. I. IRAS candidates J/A+AS/125/419 J/A+AS/125/419 Obscured AGB in Magellanic Clouds. I. Obscured AGB stars in the Magellanic Clouds. I. IRAS candidates C Loup A A Zijlstra L B F M Waters M A T Groenewegen Astron. Astrophys. Suppl. Ser. 125 419 1997 1997A&AS..125..419L Infrared sources Planetary nebulae Stars, supergiant circumstellar matter stars: AGB and post-AGB stars: late-type stars: mass-loss supergiants We have selected 198 IRAS sources in the Large Magellanic Cloud, and 11 in the Small Magellanic Cloud, which are the best candidates to be mass-loosing AGB stars (or possibly post-AGB stars). We used the catalogues of Schwering & Israel (1990, Cat. <II/181>) and Reid et al. (1990, Cat. <J/ApJ/348/98>). They are based on the IRAS pointed observations and have lower detection limits than the Point Source Catalogue. We also made cross-identifications between IRAS sources and optical catalogues.
Optically known red supergiants or AGB stars with an IRAS counterpart. Obscured AGB (without any known optical counterpart) identified as such through JHK(L) photometry Planetary nebulae with an IRAS counterpart IRAS sources from group 1, i.e. the best candidates to be AGB or post-AGB stars, or PNe. IRAS sources from group 2 : IRAS data does not allow to conclude on their nature; they can be anything Foreground stars associated with IRAS sources from groups 1 and 2 IRAS sources associated with hot stars, clusters, HII regions, or galaxies LI LI number (Schwering & Israel 1990, <II/181>) --- TRM TRM number (Reid et al. 1990, <J/ApJ/348/98>) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec S12 IRAS 12 microns flux (blank = not detected) Jy n_S12 Note on S12 (: uncertain, C contaminated) --- S25 IRAS 25 microns flux (blank = not detected) Jy n_S25 Note on S12 (: uncertain, C contaminated) --- S60 IRAS 60 microns flux (blank = not detected) Jy n_S60 Note on S12 (: uncertain, C contaminated) --- S100 IRAS 100 microns flux (blank = not detected) (no data for table4 and table5) Jy n_S100 Note on S12 (: uncertain, C contaminated) --- l_C21 Limit flag on C21 --- C21 log(12S25/25S12) --- u_C21 Uncertainty flag on C21 --- l_C32 Limit flag on C32 --- C32 log(25S60/60S25) --- u_C32 Uncertainty flag on C32 --- group group as defined in section 3. --- ident identification and comments number=1 Reference codes in brackets: a: Westerlund, 1961UppAn...5a...1W D: Westerlund et al., 1978A&AS...31...61W d: Humphreys, 1979ApJS...39..389H e: Glass, 1979MNRAS.186..317G g: Feast et al., 1980MNRAS.193..377F i: Westerlund et al., 1981A&AS...43..267W j: Catchpole & Feast, 1981MNRAS.197..385C l: Wood et al., 1983ApJ...272...99W L: Rebeirot et al., 1983A&AS...51..277R n: Glass & Reid, 1985MNRAS.214..405G o: Elias et al., 1985ApJS...57...91E q: Reid et al., 1988MNRAS.232...53R r: Lundgren, 1988A&A...200...85L v: Reid et al., 1990ApJ...348...98R, Cat. <J/ApJ/348/98> 1: Elias et al., 1986ApJ...302..675E 2: Wood et al., 1986ApJ...306L..81W 3: Whitelock et al., 1989MNRAS.238..769W 4: Reid, 1991ApJ...382..143R 5: Wood et al., 1992ApJ...397..552W 6: Roche et al., 1993MNRAS.262..301R 7: Zijlstra et al., 1996MNRAS.279...32Z Source name codes : SkKM, Sanduleak, (1989AJ.....98..825) SP, Sanduleak Philip, (1977PW&SO...2..105S) WORC, Westerlund, Olander, Richer, Crabtree, (1978A&AS...31...61W) WOH (SG for supergiants candidates in Table I, G for giants candidates in Table II), Westerlund, Olander, Hedin, (1981A&AS...43..267W) RMMP, Rebeirot, Martin, Mianes, Prevot, et al., (1983A&AS...51..277R) GRV, Reid, Glass, and Catchpole, (1988MNRAS.232...53R) SHV, Hughes, (1989AJ.....97.1634H); Hughes & Wood, (1990AJ.....99..784H) SMP comes from Sanduleak, McConnell, and Philip (1978PASP...90..621S), MG from Morgan & Good (1992A&AS...92..571M). Note to table3: We have systematically searched for IRAS counterparts of PNe listed in Meatheringham and Dopita (1991ApJS...75..407M, Cat. <J/ApJS/75/407>, 1991ApJS...76.1085M, Cat. <J/ApJS/76/1085>), Vassiliadis et al. (1992ApJS...83...87V, Cat. <J/ApJS/83/87>, 1992ApJ...394..489V), and Morgan and Good (1992A&AS...92..571M). Zijlstra et al. (1994A&A...290..228Z) find in addition IRAS counterparts to the PNe SMP 1-06, SMP 1-61, SMP 1-98, MG 45 and MA 18; these sources are not listed in Table 3 because they are located in the outer parts of the LMC and are outside the area studied by Schwering and Israel (Cat. <II/181>). --- Comparison between IRAS fluxes determinations LI LI number (Schwering & Israel 1990, <II/181>) number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- TRM TRM number (Reid et al. <J/ApJ/348/98>) number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- PSC IRAS-PSC (Cat. <II/125>) name number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S12LI IRAS 12um flux from Schwering and Israel number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy u_S12LI Uncertainty flag on S12LI number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S12TRM IRAS 12um flux from Reid et al. number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy l_S12PSC Limit flag on S12PSC number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S12PSC IRAS 12um flux from the IRAS-PSC number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy S25LI IRAS 25um flux from Schwering and Israel number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy u_S25LI Uncertainty flag on S25LI number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S25TRM IRAS 25um flux from Reid et al. number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy l_S25PSC Limit flag on S25PSC number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S25PSC IRAS 25um flux from the IRAS-PSC number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy S60LI IRAS 60um flux from Schwering and Israel number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy n_S60LI : uncertainty, C contaminated number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S60TRM IRAS 60um flux from Reid et al. number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy n_S60TRM C: contaminated number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- l_S60PSC Limit flag on S60PSC number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S60PSC IRAS 60um flux from the IRAS-PSC number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy S100LI IRAS 100um flux from Schwering and Israel number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy n_S100LI : uncertainty, C contaminated number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S100TRM IRAS 100um flux from Reid et al. C: contaminated number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy l_S100PSC Limit flag on S100PSC number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. --- S100PSC IRAS 100um flux from the IRAS-PSC number= LI-LMC 0143 : SHV0453582-690242; LI-LMC 0153 : WOH SG066 = RMMP 045 = SHV0454257-684856 LI-LMC 0253 : WOH SG097 = RMMP 087 LI-LMC 0383 : WOH SG140 = SP 29-33 = RMMP 151 LI-LMC 0425 : WOH SG157 = RMMP 183 LI-LMC 0517 : SP 35-1 = WOH SG179 = RMMP 215 LI-LMC 0612 : SP 37-24 = WOH SG193 = RMMP 239 LI-LMC 0663 : SP 37-35 = WOH SG204 = RMMP 256 LI-LMC 0869 : SP 47-6 = WOH SG241 = RMMP 308 LI-LMC 0932 : WOH SG257 LI-LMC 0976 : RMMP 339 LI-LMC 1038 : RMMP 358 LI-LMC 1059 : SP 46-16 = WOH SG287 = RMMP 364 TRM 052 : SP 45-16 = WOH SG299 = RMMP 383 TRM 073 : SP 45-18 = WOH SG301 = RMMP 384 LI-LMC 1103 : WOH SG306 = RMMP 390 LI-LMC 1107 : HV 5854 = SP 45-23 = WOH SG313 = RMMP 401 LI-LMC 1125 : SP 46-32 = WOH SG319 = RMMP 408 LI-LMC 1145 : SP 47-17 = WOH SG331 = RMMP 432 LI-LMC 1155 : WOH SG337 = RMMP 444 LI-LMC 1163 : SP 46-39 = WOH SG338 = RMMP 448 LI-LMC 1170 : WOH SG343 = RMMP 468 = R 108 LI-LMC 1172 : WOH SG341 = RMMP 462 LI-LMC 1190 : SP 45-38 = WOH SG349 = RMMP 482 LI-LMC 1212 : SP 47-20 = WOH SG358 = RMMP 505 LI-LMC 1223 : SP 47-22 = WOH SG369 = RMMP 519 LI-LMC 1234 : SP 51-6 = WOH SG371 = RMMP 531 LI-LMC 1238 : RMMP 539 LI-LMC 1241 : WOH SG375 = RMMP 545 LI-LMC 1281 : SP 46-59 = WOH SG388 = RMMP 575 LI-LMC 1294 : WOH SG395 = RMMP 589 = GRV0533-6650 LI-LMC 1304 : SP 52-18 = WOH SG401 = RMMP 606 LI-LMC 1360 : SP 52-29 = WOH SG422 = RMMP 656 LI-LMC 1364 : WOH SG421 = RMMP 655 LI-LMC 1366 : SP 52-32 ?? LI-LMC 1399 : SP 52-35 = WOH SG432 = RMMP 683 LI-LMC 1553 : SP 54-34 = WOH SG467 = RMMP 753 LI-LMC 1559 : SP 54-40 = WOH SG473 = RMMP 761 WOH G352 : also very close to LI-LMC 1125. LI-SMC 61 = PSC00483-7347. Was not selected because it is mentioned as slightly extended in Schwering & Israel (Cat. <II/181>); note that Whitelock et al. (1989MNRAS.238..769W) mention that this object could also be a pre-main-sequence star. LI-LMC 1341 : near a nebulosity. LI-SMC 233 : Galaxy or PN ? (3 reference for each ...) LI-SMC 48 : near LHA 115-S 9 (B1, V=14.0), and RAW 479 (C:, V=16.3) LI-LMC 197 : near the G4Ia supergiant HD 268759 but only very rough coordinates are available LI-LMC 203 : near SK-69 39a (A3Iab, B=12.5) and HV 12501 (M1.5, V=11.9) LI-LMC 493 : near BMB-BW49=BM 16-24 (C, I=14.0) LI-LMC 530 : near SHV0510004-692755 (M6, I=14.7, P=169) LI-LMC 568 : could be associated with IRAS-PSC 05112-6843 LI-LMC 595 : near BM 18-8 and 18-9 (C) LI-LMC 644 : near HV 2378 LI-LMC 696 : near BM 20-13 (C) LI-LMC 730 : near BM 21-13 (C) LI-LMC 825 : could be associated with IRAS-PSC 05205-6913 LI-LMC 987 : near HD 269507 (K, B=11.5) but only very rough coordinates are available. Could be associated with IRAS-PSC 05249-6916. LI-LMC 1028 : near BM 23-21 (C) LI-LMC 1055 : near SK-67 109 (V=13.1) LI-LMC 1082 : near SK-66 97 (B=12.5) and SK-66 98 (B=11.9) LI-LMC 1378 : near BM 33-31 (C) LI-LMC 1657 : near BM 37-32 (C) LI-LMC 1775 : near WORC 220 (C) LI-LMC 1785 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 1795 : a bright R counterpart is found by Zijlstra et al. (1996MNRAS.279...32Z) LI-LMC 1807 = IRAS-PSC06011-6636A LI-SMC 19 : near RAW 179 (C, V=16.8) LI-SMC 72 : near RAW 651 (C, V=17.3), RAW 658 (C, V=17.6), and the cepheid HV 1522 (V=14.6) LI-SMC 78 : in a cluster ? Near RAW 706 (C, V=17.0) LI-SMC 96 : 96 and 97 are probably the same IRAS source. Near RAW 822 (C, V=17.6), AzV 148 (B0, V=14.3), and the Cepheid HV 1598 (V=15.9) LI-SMC 100 : near RAW 832 (C, V=17.3) LI-SMC 106 : near RAW 941 (C, V=17), the Cepheid HV 1649 (V=15.5), and the foreground red variable Z Tuc (B=13) LI-SMC 112 : near the foreground star HV 5627 (F7V, V=9.5) LI-SMC 133 : near the known or suspected KM supergiants SkKM 187, SkKM 190, HV 11402, and PMMR 100 (M0.5, V=12.8) LI-SMC 143 : near RAW 1258 (C, V=16.9) and RAW 1254 (C, V=17.1) TRM 137 : near HD 268931 (G, B=12.2) and HD 268933 (F, B=12.2) but only very rough coordinates are available LI-LMC 1839 : AGN candidate in De Grijp et al. (1987A&AS...70...95D) LI-LMC 478 : According to Israel & Koorneef (1991A&A...248..404I), there is a M giant or supergiant near the IRAS position. However the association is doubtful LI-LMC 435 : near the cepheid HV 893 LI-LMC 531 : near the M supergiant HV 5625 (V=12.6) and the B5Iab supergiant HD 269101 (V=12.0) LI-LMC 541 : near BMB-BW097 (M6, I=14.0) LI-LMC 718 : near BM 21-10=SP 38-16 (C) LI-LMC 794 = IRAS-PSC 05191-6936. Near the C star SHV0518595-693653 LI-LMC 832 : near the M6 star SHV0520342-693911 LI-LMC 1010 : near the IRAS extended structure X0525-662 LI-LMC 1094 : near the IRAS extended structure X0527-714 LI-LMC 1292 : near a nebulosity LI-LMC 1315 : could be associated with IRAS-PSC 05338-6725 LI-LMC 1336 : near HD 269762 (B9Ia, V=11.4), HV 2677 (M3/5, V=13.6), and the PN SMP 1-78 LI-LMC 1390 : near BM 33-37 and BM 33-43 (C) LI-LMC 1434 : could be associated with IRAS-PSC 05375-6949 LI-LMC 1494 : could be associated with IRAS-PSC 05399-6906 LI-LMC 1535 : near BM 36-7 (C) LI-SMC 90 : could be identified with IRAS 00515-7455; LI-LMC 147 : could be identified with IRAS 04544-6722; LI-LMC 838 : could be identified with IRAS 05209-7101; LI-LMC 1812 = IRAS 06024-6645A. LI-LMC 1130 : Zijlstra et al. (paper II, 1996MNRAS.279...32Z) find a bright R counterpart (SP 44-29), and Reid et al. (1990, Cat. <J/ApJ/348/98>) find 2 possible optical identifications; the infrared colours indicate that the star is not obscured; either the star is not associated with the IRAS source (Zijlstra et al.), either it is a hot star, or it is embedded in a nebula. Jy Patricia Bauer CDS 1997 Feb 12 Cecile Loup <loup@condrieu.iap.fr> J_A+AS_125_419.xml Stellar models for a wide range of initial chemical compositions until helium burning. III. From X=0.55 to X=0.75, for Z=0.03 J/A+AS/125/439 J/A+AS/125/439 Stellar models until He burning - III. Stellar models for a wide range of initial chemical compositions until helium burning. III. From X=0.55 to X=0.75, for Z=0.03 A Claret Astron. Astrophys. Suppl. Ser. 125 439 1997 1997A&AS..125..439C J/A+AS/109/441 : Stellar models until He burning - I. (Claret, 1995) J/A+AS/114/549 : Stellar models until He burning - II. (Claret+, 1995) Models, evolutionary apsidal motion binaries: general chemical composition stars: evolution In this Paper I present grids for the stellar models with a slightly higher metallic content than in the previous works (Claret, 1995A&AS..109..441C; Claret & Gimenez, 1995A&AS..114..549C), say, Z=0.03. The initial helium abundances in mass are Y_i_=0.42, 0.32 and 0.22; this last value was used only to facilitate interpolations since it is a little bit smaller than the primordial helium abundance. The present computations are based on the radiative opacities with spin-orbi t coupling provided by the Lawrence Livermore group (Iglesias et al., 1992ApJ...397...71I). For the lower temperatures I have used the results by Alexander (1992, priv. comm.). Core overshooting was taken into account as well as mass loss. The models presented here cover the mass range between 1 and 40M_{sun}_. I also compute for all models the internal structure constants k_j_ and the radius of gyration {beta}. For the first time the calculation of the tidal constants E_2_ and {lambda}_2_, which are used to evaluate circularization and synchronization times in binary stars, are presented for stellar models as a function of the initial mass and time. The former is related with the dynamical tidal contribution to the total perturbed potential in a binary star while the latter is connected with the external structure of the outer layers.
All models with Z=0.03, X=0.55, 0.65 and 0.75 logM Initial mass of the model [solMass] X X initial composition (H) --- Z Z initial composition --- Overshoot without (0) or with (1) overshooting --- Age Age of models yr log(L) Total luminosity [solLum] log(g) Surface gravity [cm/s2] log(Teff) Effective temperature [K] log(k2) Apsidal motion constant (j=2) --- log(k3) Apsidal motion constant (j=3) --- log(k4) Apsidal motion constant (j=4) --- alpha alpha = -E_p_ x R/GM^2 --- beta Fractional gyration radius ---- Patricia Bauer CDS 1997 Apr 17 A. Claret <claret@iaa.es> J_A+AS_125_439.xml Properties of nearby clusters of galaxies. III: A 76, A 157, A 407, A 505, A 671, A 779, A 1700, A 2028, A 2040, A 2052, A 2063, A 2065, A 2593, A 2657, A 2670 J/A+AS/125/459 J/A+AS/125/459 Nearby clusters of galaxies properties. III. Properties of nearby clusters of galaxies. III: A 76, A 157, A 407, A 505, A 671, A 779, A 1700, A 2028, A 2040, A 2052, A 2063, A 2065, A 2593, A 2657, A 2670 D Trevese G Cirimele A Cenci B Appodia P Flin P Hickson Astron. Astrophys. Suppl. Ser. 125 459 1997 1997A&AS..125..459T J/A+AS/94/327 : Nearby clusters of galaxies. I. (Trevese+ 1992) J/A+AS/110/313 : Clusters of galaxies properties. II. (Flin+ 1995) Clusters, galaxy Photometry galaxies: clusters: general This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. <J/A+AS/94/327>, Flin et al. 1995, Cat. <J/A+AS/110/313>, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.
*Coordinates, size, ellipticity, position angle, total and aperture magnitudes of galaxies in the field of Abell clusters Abell Abell cluster name --- ID Identification galaxy number --- m_ID Multiplicity index on N number=1 The data of Table 2 have been included, with galaxy identification number 4a and 4b to maintain the identification of pap.I unchanged. --- RAh Right ascension 2000 h RAm Right ascension 2000 min RAs Right ascension 2000 s DE- DEclination sign --- DEd Declination 2000 (including sign) deg DEm Declination 2000 arcmin DEs Declination 2000 arcsec R1 Aperture radius for total magnitude number=2 R1=1.5r1 where r1 = [int(0,rmax)I(r)r^2^dr]/[int(0,rmax)I(r)rdr] see Kron R.G., 1980ApJS...43..305K arcsec Eps Ellipticity --- Theta Position angle (from north, counterclockwise) deg magTot Total apparent F magnitude (within R1) mag magApp Apparent magnitude in a fixed aperture (PHIa as defined in Table 1) mag Multip s: star, d: double object --- T92 Label on Trevese (1992A&AS...94..327T) identification map number=3 This field has been added to Abell 1185 and Abell 1213 data to correct the mismatch between the sequential number in table and in the identification map of pap. I. --- tables.tex LaTeX version of tables 3 to 17 tables.ps PostScript version of tables 3 to 17 Patricia Bauer CDS 1998 Sep 08 Dario Trevese <trevese@astrm2.rm.astro.it> UNKNOWN UNKNOWN * 10-Mar-1997: first version. * 08-Sep-1998: the following modifications have been made: For A 1213 and A 1775 absolute coordinates RA and DE have been revised; in the case of A 407, A 1185, A 1775, A 1213, A 2053, A 2063, A 2319, A 2593, A 2597 an `s' or `d' has been added to indicate stars or double object respectively, and some unreliable data corresponding to faint objects very close to bright ones have been erased. For A 1185 and A 1213 a label to correctly identify the objects on the map in Trevese et al., 1992 (Cat. <J/A+AS/94/327>) has been added. J_A+AS_125_459.xml Four-colour photometry of eclipsing binaries. XXXVIII. Light curves of the triple system V906 Scorpii J/A+AS/125/471 J/A+AS/125/471 Light curves of the triple system V906 Sco Four-colour photometry of eclipsing binaries. XXXVIII. Light curves of the triple system V906 Scorpii L P R Vaz J Andersen J V Clausen B E Helt J M Garcia A Gimenez S H P Alencar Astron. Astrophys. Suppl. Ser. 125 471 1997 1997A&AS..125..471V J/A+AS/101/49 : V Crateris ubvy photometry (Liu 1993) J/A+AS/101/563 : GG Lupi ubvy photometry (Clausen+ 1993) J/A+AS/109/425 : AO Velorum ubvy photometry (Clausen+ 1995) J/A+AS/112/123 : LZ Centauri ubvy photometry (Vaz+ 1995) J/A+AS/115/315 : V539 Arae ubvy photometry (Clausen+ 1996) Alencar S.H.P., Vaz L.P.R., Helt B.E., 1997A&A...326..709A Binaries, eclipsing Photometry, uvby binaries: eclipsing stars: individual (V906 Sco) Complete uvby light curves of the detached triple-lined late B-type eclipsing binary V906 Scorpii, obtained from 1987 to 1991, are presented. A detailed photometric analysis based on these observations and on new spectroscopic material yields accurate masses and radii (errors <2%) for the components, confirms that the system is member of NGC 6475 (Messier 7) and is published separately (Alencar et al., 1997A&A...326..709A)
V906 Sco HD 162724 17 53 54.7 -34 45 09 HD 162631 17 53 34.8 -34 51 55
Magnitude differences V906 Sco - HD 162631 obtained from 1987 to 1991 (instrumental system) HJD Heliocentric Julian Day d ymag Magnitude y mag b-y Colour index b-y mag m1 Stroemgren index m1 mag c1 Stroemgren index c1 mag bmag Magnitude b mag vmag Magnitude v mag umag Magnitude u mag Patricia Bauer CDS 1997 Apr 01 Luiz Paulo R. Vaz <vaz@suya.fisica.ufmg.br> J_A+AS_125_471.xml On the possible variability of the main sequence A stars theta Virginis and 109 Virginis J/A+AS/125/497 J/A+AS/125/497 Theta Vir and 109 Vir uvby photometry On the possible variability of the main sequence A stars theta Virginis and 109 Virginis S J Adelman Astron. Astrophys. Suppl. Ser. 125 497 1997 1997A&AS..125..497A J/A+AS/103/1 : 63 And, HD 192913, HR 8240 & 108 Aqr (Adelman+ 1994) J/A+AS/106/333 : Alpha And, HD 184905, HR 8216 & HR 8434 (Adelman+ 1994) J/A+AS/114/253 : HD 11187, HD 14940, HD 15144, 20 Eri, HR 8933 (Adelman+ 1995) J/A+AS/122/249 : HD 32633, 25 Sex, HR 7224 & HD 200311 (Adelman, 1997) J/A+AS/125/65 : HD 37776, HR 2258, HR 6958 & 108 Aqr (Adelman, 1997) J/PASP/109/9 : HR 1643, Theta Aur, 49 Cam, and HR 3724 (Adelman 1997) Photometry, uvby Stars, A-type Stars, dwarfs stars: individual (theta Vir, 109 Vir) stars: variables: other Differential Stroemgren uvby photometric observations from the Four College Automated Photoelectric Telescope are used to examine the possible variability of the spectrophotometric standards {theta} Vir and 109 Vir. No evidence is found for variability within a season of observation. Small year to year differences are most likely due to unaccounted for extinction changes.
theta Vir HD 114330 13 09 57.0 -05 32 18 * 109 Vir HD 130109 14 46 15.2 +01 53 36
uvby Photometry of Theta Vir Examination of Data on Nights for Theta Vir uvby Photometry of 109 Vir Examination of Data on Nights for 109 Vir HJD Heliocentric Julian Date d u(v-c) variable-comparison (v-c) u magnitude mag u(ch-c) check-comparison (ch-c) u magnitude mag v(v-c) variable-comparison (v-c) v magnitude mag v(ch-c) check-comparison (ch-c) v magnitude mag b(v-c) variable-comparison (v-c) b magnitude mag b(ch-c) check-comparison (ch-c) b magnitude mag y(v-c) variable-comparison (v-c) y magnitude mag y(ch-c) check-comparison (ch-c) y magnitude mag Averaged values Star Star name --- Per Period considered number=1 For Theta Vir : year2: from 2448732.7901 to 2448807.6543 year3: from 2449008.9258 to 2449146.7282 year4: from 2449335.0287 to 2449476.8279 year5: from 2449736.0539 to 2449855.7760 For 109 Vir : year2: from 2448679.9591 to 2448765.7706 year3: from 2449009.9714 to 2449150.7427 year4: from 2449412.8808 to 2449502.7557 year5: from 2449746.9679 to 2449867.8048 For night averaged data: Per = HJD of the night of observation. Nyear4 : year 4 average 5 or more observations/night Nyear5 : average 5 or more observations/night --- u(v-c) variable-comparison (v-c) u magnitude mag e_u(v-c) rms uncertainty on (v-c) u magnitude mag u(ch-c) check-comparison (ch-c) u magnitude mag e_u(ch-c) rms uncertainty on (ch-c) u magnitude mag v(v-c) variable-comparison (v-c) v magnitude mag e_v(v-c) rms uncertainty on (v-c) v magnitude mag v(ch-c) check-comparison (ch-c) v magnitude mag e_v(ch-c) rms uncertainty on (ch-c) v magnitude mag b(v-c) variable-comparison (v-c) b magnitude mag e_b(v-c) rms uncertainty on (v-c) b magnitude mag b(ch-c) check-comparison (ch-c) b magnitude mag e_b(ch-c) rms uncertainty on (ch-c) b magnitude mag y(v-c) variable-comparison (v-c) y magnitude mag e_y(v-c) rms uncertainty on (v-c) y magnitude mag y(ch-c) check-comparison (ch-c) y magnitude mag e_y(ch-c) rms uncertainty on (ch-c) y magnitude mag Patricia Bauer CDS 1997 Feb 03 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> UNKNOWN UNKNOWN There were an inversion between the b and v magnitude labels. This was corrected on 24-Apr-1998 J_A+AS_125_497.xml Atomic data for interpretation of HgMn spectra: transition probabilities of Mn III J/A+AS/125/539 J/A+AS/125/539 Mn III position probabilities Atomic data for interpretation of HgMn spectra: transition probabilities of Mn III P H M Uylings A J J Raassen Astron. Astrophys. Suppl. Ser. 125 539 1997 1997A&AS..125..539U Atomic physics atomic data stars: chemically peculiar Transition probabilities of the spectrum of Mn III are calculated using the orthogonal operator description for both the odd and the even energy levels.
*log(gf) values for the 3d^5+3d^4 4s-->3d^4 4p electric dipole (E1) transitions lambda Wavelength number=1 Wavelength obtained from the energy differences between the experimental level values. Wavelengths below 2000 Angstrom are given as vacuum wavelengths and above 2000 Angstrom as air wavelengths. 0.1nm log(gf) Oscillator strength --- Jf J-value final state --- Ef Energy value final state cm-1 n_Ef Indication known/unknown number=2 An '*' after the energy value indicates that the level is known, in which case the experimental level value is given. When unknown, the calculated energy value is given and used to approximate the wavelength. --- Lf Leading term final state number=3 The first character of the level name designates the configuration number: for the even levels '1' refers to 3d^5 and '2' to 3d^4 4s; for the odd levels '1' refers to 3d^4 4p. --- Ji J-value initial state --- Ei Energy value initial state cm-1 n_Ei Indication known/unknown number=2 An '*' after the energy value indicates that the level is known, in which case the experimental level value is given. When unknown, the calculated energy value is given and used to approximate the wavelength. --- Li Leading term initial state number=3 The first character of the level name designates the configuration number: for the even levels '1' refers to 3d^5 and '2' to 3d^4 4s; for the odd levels '1' refers to 3d^4 4p. --- A-values for the forbidden lines lambda Wavelength 0.1nm AM1 A-value (M1) number=1 The A-values for the forbidden lines given are restricted to the magnetic dipole (M1) and electric quadrupole (E2) transitions within the 3d^5+3d^4 4s configurations, from levels with an energy of less than 75,000cm^-1^ above the ground and with A-values larger than 10^-3^s^-1^. s-1 AE2 A-value (E2) number=1 The A-values for the forbidden lines given are restricted to the magnetic dipole (M1) and electric quadrupole (E2) transitions within the 3d^5+3d^4 4s configurations, from levels with an energy of less than 75,000cm^-1^ above the ground and with A-values larger than 10^-3^s^-1^. s-1 Jf J-value final state number=2 The level with the lower J-value is given first in the designation of the transition. --- Ef Energy value final state cm-1 n_Ef Indication known/unknown number=3 An '*' after the energy value indicates that the level is known, in which case the experimental level value is given. When unknown, the calculated energy value is given and used to approximate the wavelength. --- Lf Leading term final state number=4 The first character of the level name designates the configuration number: for the even levels '1' refers to 3d^5 and '2' to 3d^4 4s. --- Ji J-value initial state number=2 The level with the lower J-value is given first in the designation of the transition. --- Ei Energy value initial state cm-1 n_Ei Indication known/unknown number=3 An '*' after the energy value indicates that the level is known, in which case the experimental level value is given. When unknown, the calculated energy value is given and used to approximate the wavelength. --- Li Leading term initial state number=4 The first character of the level name designates the configuration number: for the even levels '1' refers to 3d^5 and '2' to 3d^4 4s. --- Patricia Bauer CDS 1997 Apr 08 P. Uylings <uylings@phys.uva.nl> J_A+AS_125_539.xml Effective collision strengths for electron-impact excitation of nitrogen-like Mg VI J/A+AS/125/543 J/A+AS/125/543 Effective collision strengths for Mg VI Effective collision strengths for electron-impact excitation of nitrogen-like Mg VI C A Ramsbottom K L Bell Astron. Astrophys. Suppl. Ser. 125 543 1997 1997A&AS..125..543R Atomic physics atomic data atomic processes The effective collision strengths are presented in this table for all transitions among the lowest 23 fine-structure levels of Mg VI. Each fine-structure level is assigned an index number in Table 3 of the manuscript ranging from 1 to 23. These index values are reproduced here in Table 5 to depict a particular transition. eg. Index 1-3 denotes the transition 2s(2)2p(3)4SO(3/2)-2s(2)2p(3)2DO(5/2) The effective collision strengths for each transition are presented in rows for a number of electron temperatures ranging from log(T)=5.0 to log(T)=6.1. A superscript indicates the power of 10 by which the number should be multiplied.
Effective collision strengths for Mg VI INDEX Index numbers denoting a transition --- ECS5.0 Effective collision at log(T)=5.0 --- ECS5.1 Effective collision at log(T)=5.1 --- ECS5.2 Effective collision at log(T)=5.2 --- ECS5.3 Effective collision at log(T)=5.3 --- ECS5.4 Effective collision at log(T)=5.4 --- ECS5.5 Effective collision at log(T)=5.5 --- ECS5.6 Effective collision at log(T)=5.6 --- ECS5.7 Effective collision at log(T)=5.7 --- ECS5.8 Effective collision at log(T)=5.8 --- ECS5.9 Effective collision at log(T)=5.9 --- ECS6.0 Effective collision at log(T)=6.0 --- ECS6.1 Effective collision at log(T)=6.1 --- table5.tex LaTeX version of the table Patricia Bauer CDS 1997 Feb 28 Cathy Ramsbottom <C.Ramsbottom@Queens-Belfast.AC.UK> J_A+AS_125_543.xml uvby Photometry of the magnetic Chemically Peculiar Stars HD 37776, HR 2258, HR 6958, and 108 Aquarii J/A+AS/125/65 J/A+AS/125/65 uvby photometry of 4 CP stars uvby Photometry of the magnetic Chemically Peculiar Stars HD 37776, HR 2258, HR 6958, and 108 Aquarii S J Adelman Astron. Astrophys. Suppl. Ser. 125 65 1997 1997A&AS..125...65A J/A+AS/103/1 : 63 And, HD 192913, HR 8240 & 108 Aqr (Adelman+ 1994) J/A+AS/106/333 : Alpha And, HD 184905, HR 8216 & HR 8434 (Adelman+ 1994) J/A+AS/114/253 : HD11187, HD14940, HD15144, 20 Eri & HR8933 (Adelman+, 1995) J/A+AS/122/249 : HD 32633, 25 Sex, HR 7224 & HD 200311 (Adelman, 1997) J/PASP/109/9 : HR 1643, Theta Aur, 49 Cam, and HR 3724 (Adelman 1997) J/A+AS/125/497 : Theta Vir and 109 Vir uvby photometry (Adelman 1997) Photometry, uvby Stars, early-type Stars, peculiar stars: chemically peculiar stars: individual (108 Aqr, HD 37776, HR 2258, HR 6958) stars: variables: general Differential Stroemgren uvby photometric observations from the Four College Automated Photoelectric Telescope are presented for four magnetic chemically peculiar stars. Comparison with uvby photometry of Pedersen & Thomsen for HD 37776 yields an improved period of 1.538675 days. New periods of 15.0305 days and 18.065 days are found for the sharp-lined stars HR 2258 and HR 6958, respectively, rather than one of their aliases. For HR 6958 each color shows a slightly different time of maximum. Comparison of the four color photometry of 108 Aqr taken during the fall of 1995 which well covers the period shows the presence of a secondary minimum near primary maximum in u, v, and b. Comparison with published photometry indicates indicates that subtle changes in the shapes of the light curves have occurred suggesting that this star might be precessing.
HD 37776 V901 Ori 05 40 56.3 -01 30 26 HR 2258 HD 43819 V1155 Ori 06 19 01.8 +17 19 31 HR 6958 HD 170973 MV Ser 18 32 06.8 +03 39 35 HD 223640 108 Aqr HR 9031 ET Aqr 23 51 21.1 -18 54 33
uvby Photometry for HD 37776 uvby Photometry for HR 2258 uvby Photometry for HR 6958 uvby Photometry for 108 Aqr HJD Heliocentric Julian Date d umag1 Variable-comparison (v-c) u magnitude mag umag2 Check-comparison (ch-c) u magnitude mag vmag1 Variable-comparison (v-c) v magnitude mag vmag2 Check-comparison (ch-c) v magnitude mag bmag1 Variable-comparison (v-c) b magnitude mag bmag2 Check-comparison (ch-c) b magnitude mag ymag1 Variable-comparison (v-c) y magnitude mag ymag2 Check-comparison (ch-c) y magnitude mag Average photometry Name star name --- Per Period considered number=1 For HD 37776 : year5: From 2449702.7198 to 2449797.6208 year6: From 2449990.9415 to 2450130.6660 For HR 2258 : year2: From 2448561.9920 to 2448705.6274 year3: From 2448938.9820 to 2449072.6335 year4: From 2449292.8755 to 2449424.6660 year5: From 2449646.9987 to 2449805.6279 year6: From 2450035.9458 to 2450175.6183 For HR 6958 : year1: From 2448333.0098 to 2448441.7875 year2: From 2448530.6068 to 2448808.7655 year3: From 2448873.6732 to 2449167.8855 year4: From 2449413.0234 to 2449548.7582 year5: From 2449548.7582 to 2449901.8472 --- umag1 Variable-comparison (v-c) u magnitude mag e_umag1 rms uncertainty on umag1 mag umag2 Check-comparison (ch-c) u magnitude mag e_umag2 rms uncertainty on umag2 mag vmag1 Variable-comparison (v-c) v magnitude mag e_vmag1 rms uncertainty on vmag1 mag vmag2 Check-comparison (ch-c) v magnitude mag e_vmag2 rms uncertainty on vmag2 mag bmag1 Variable-comparison (v-c) b magnitude mag e_bmag1 rms uncertainty on bmag1 mag bmag2 Check-comparison (ch-c) b magnitude mag e_bmag2 rms uncertainty on bmag2 mag ymag1 Variable-comparison (v-c) y magnitude mag e_ymag1 rms uncertainty on ymag1 mag ymag2 Check-comparison (ch-c) y magnitude mag e_ymag2 rms uncertainty on ymag2 mag Patricia Bauer CDS 1996 Dec 20 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> UNKNOWN UNKNOWN There were an inversion between the b and v magnitude labels. This was corrected on 24-Apr-1998 J_A+AS_125_65.xml UBV photometry of Be stars at Hvar: 1972-1990 J/A+AS/125/75 J/A+AS/125/75 UBV photometry of Be stars UBV photometry of Be stars at Hvar: 1972-1990 K Pavlovski P Harmanec H Bozic P Koubsky P Hadrava S Kriz Z Ruzic S Stefl Astron. Astrophys. Suppl. Ser. 125 75 1997 1997A&AS..125...75P Photometry, UBV Stars, Be stars: emission-line, Be stars: individual (omicron Cas, QR Vul) stars: variables: general A summary of results of the systematic UBV photoelectric monitoring of bright northern Be stars carried out at the Hvar Observatory between 1972 and 1990 is presented. Altogether, 76 Be stars of all luminosity classes were observed and 13848 UBV measurements secured. Simultaneously, 9648 UBV measurements of 48 check stars (most of them of early spectral types) were obtained. A careful transformation of all observations into the standard Johnson system allowed detection and monitoring of even very mild long-term light and colour variations of these objects. Almost all early-type Be stars in the sample turned out to be variable. For several stars phase-locked light variations related to their binary nature were established. Sudden brightenings, on a time scale of a few days, were detected for o Cas and QR Vul.
omicron Cas HD 4180 00 44 43.4 +48 17 04 QR Vul HD 192685 20 15 15.8 +25 35 31
List of the comparison stars HD HD (Cat. <III/135>) number --- Name Other name of star --- Vmag Johnson V magnitude mag B-V Johnson B-V index mag U-B Johnson U-B index mag SpType Spectral type --- List of the check stars HD HD (Cat. <III/135>) number --- Name Other name of star --- Season Number of seasons yr o_Vmag Number of UBV measurements --- Vmag Johnson V magnitude mag e_Vmag Standard deviation in Vmag mag Bmag Johnson B magnitude mag e_Bmag Standard deviation in Bmag mag Umag Johnson U magnitude mag e_Umag Standard deviation in Umag mag SpType Spectral type --- Patricia Bauer CDS 1997 Sep 09 Kresimir Pavlovski <kresimir@geof.hr> J_A+AS_125_75.xml Kinematical data on early-type galaxies. II. J/A+AS/126/15 J/A+AS/126/15 Kinematical data on early-type galaxies. II. Kinematical data on early-type galaxies. II. F Simien P Prugniel Astron. Astrophys. Suppl. Ser. 126 15 1997 1997A&AS..126...15S J/A+AS/122/521 : Kinematical data on early-type galaxies. I. (Simien+ 1997) J/A+AS/126/519 : Kinematical data on early-type galaxies. III. (Simien+ 1997) Galaxies, rotation Radial velocities Velocity dispersion galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: general galaxies: kinematics and dynamics We present new kinematical data for a sample of 38 early-type galaxies. Rotation curves and velocity-dispersion profiles are determined for 32 objects, while the central velocity dispersions are given for the whole sample. This is our second paper in a series devoted to the presentation of kinematical data on elliptical and S0 galaxies, derived from long-slit absorption spectroscopy.
Catalog elements for program galaxies Name Object identification number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) --- MType Morphological type number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) --- RAh Right Ascension 1950 (hours) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) h RAm Right Ascension 1950 (minutes) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) min RAs Right Ascension 1950 (seconds) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) s DE- Declination 1950 (sign) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) --- DEd Declination 1950 (degrees) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) deg DEm Declination 1950 (minutes) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) arcmin DEs Declination 1950 (seconds) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) arcsec RV Heliocentric radial velocity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) km/s BT Integrated blue magnitude number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) mag Dist Distance modulus number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) mag Re Effective radius number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) arcsec Eps Ellipticity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) --- PA Position angle of slit PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) deg r_Eps Reference for Eps and PA 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) --- Sig0 Central velocity dispersion number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) km/s e_Sig0 Error on Sig0 number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) km/s Vmax Maximum rotational velocity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) km/s e_Vmax Error on Vmax number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = LEDA (status: LEDA1996) km/s Log of the observations Name Object identification number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). --- Date Date of observation number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). "DD/MM/YY" PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). deg Nexp Number of exposures number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). --- Texp Exposure time number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). min Seeing Seeing FWHM number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). arcsec u_Seeing uncertainty flag on Seeing number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). --- Kinematical results (mostly central values) Name Object identification --- Vhel Heliocentric radial velocity km/s u_Vhel Uncertainty flag on Vhel --- e_Vhel Mean error on Vhel km/s sig0 Central velocity dispersion number=1 rotation and dispersion velocities are projected along the line of sight km/s u_sig0 Uncertainty flag on sig0 --- e_sig0 Mean error on sig0 km/s l_Vmax Upper-limit flag on Vmax --- Vmax Maximum rotational velocity number=1 rotation and dispersion velocities are projected along the line of sight km/s u_Vmax Uncertainty flag on Vmax --- e_Vmax Mean error on Vmax km/s rmax Radius corresponding to Vmax arcsec Profiles of velocity dispersion and rotation Name Object identification number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. --- PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg r Radius (<0 and >0 on opposite semi-axes) number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. arcsec Vrot Projected mean stellar rotation velocity Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s e_Vrot Mean error on Vrot number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s sigma Projected velocity dispersion number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s e_sigma Mean error on sigma number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s Francois Simien CRAL 1997 Jun 09 Francois SIMIEN <fs@cumulus.univ-lyon1.fr> UNKNOWN UNKNOWN With respect to the printed version of the graphs, a change can be noticed in the PA angles of a few galaxies (table4): this is due to a new convention which is applied, starting with the printed version of Paper III (in press), and which is aimed at suppressing an uncertainty of 180 degrees on these angles. The convention is explained, below, as notes to the files table2 and table4. The changes are for the following galaxies: NGC 1521, 2332, 3921, 4435, 4464, 4479, and 4874, and UGC 3792. J_A+AS_126_15.xml Measurements of double stars made at Nice Observatory with the 74 and 50 cm refractors J/A+AS/126/1 J/A+AS/126/1 Double stars measurements Measurements of double stars made at Nice Observatory with the 74 and 50 cm refractors R Gili P Couteau Astron. Astrophys. Suppl. Ser. 126 1 1997 1997A&AS..126....1G J/A+AS/106/377 : Double star measurements (Couteau+, 1994) I/209 : Catalogue of 2700 double stars (Couteau, 1995) Stars, double and multiple astrometry binaries: visual We give 657 measurements of double stars, Table 1 by R. Gili with CCD camera, Table 2 by P. Couteau with filar micrometer.
CCD camera measurements (by R. Gili) Ident ADS, BD, AGK2 or AC identification --- Name Binary name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin Vmag Total V magnitude mag Ep-1900 Observation epoch (1900+) yr Theta Position angle deg l_rho Limit flag on rho --- rho Separation angle deg l_md Limit flag on md --- md Magnitude difference mag Q Quadrant indication number=1 1Q = first quadrant, 2Q = second quadrant 3Q = third quadrant, 4Q = last quadrant --- u_Q Uncertainty flag on Q --- Tel Telescope (50cm or 74cm) -- n_Tel --- Note Notes --- Filar micrometre measurements (by P. Couteau) Ident. BD, AC or ADS identification --- Name Binary name --- Vmag Visual magnitude mag RAh Right ascension (J2000) h RAm Right ascension (J2000) min DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin Ep-1900 Observation epoch (+1900) yr Theta Position angle deg n_Theta S fot Simple, : uncertainty flag --- rho Separation angle deg md Difference magnitude mag Q Quadrant --- Nobs Observation nights number followed by N for 74cm instrument and n for 50cm instrument --- Note Notes --- Patricia Bauer CDS 1997 Feb 28 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_126_1.xml Radial velocities, rotations, and duplicity of a sample of early F-type dwarfs J/A+AS/126/21 J/A+AS/126/21 Velocities and duplicity of F-type dwarfs Radial velocities, rotations, and duplicity of a sample of early F-type dwarfs B Nordstroem R P Stefanik D W Latham J Andersen Astron. Astrophys. Suppl. Ser. 126 21 1997 1997A&AS..126...21N Radial velocities Rotational velocities Stars, dwarfs binaries: spectroscopic methods: statistical solar neighborhood stars: kinematics techniques: radial velocities We present new radial and rotational velocities for 595 nearby early F dwarfs, based on digital spectra cross-correlated with individually optimised synthetic template spectra. The selection of optimum templates, the determination of rotational velocities, and the extraction of velocities from the blended spectra of double-lined spectroscopic binaries are discussed in some detail. We find 170 spectroscopic binaries in the sample and determine orbits for 18 double-lined and 2 single-lined binaries, including some spectroscopic triples. 73 stars are listed with too rapid rotation to yield useful radial velocities (i.e. vsini>120km/s). We discuss the binary frequency in the sample, and the influence of unrecognised binaries on the definition of clean metallicity groups of young F dwarfs and the determination of their kinematical properties.
Mean radial velocities, mean errors, and variability indicators for 530 stars with single-lined spectra HD HD number of single-lined star --- m_HD Visual binary component code --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Teff Effective temperature (Template spectrum parameter) K logg Surface gravity (Template spectrum parameter) [mm/s2] Vrot Estimated rotational velocity, v sin i km/s Nobs Number of observations --- Span Time span from first to last observation d <RV> Mean radial velocity km/s e_<RV> Mean error of mean radial velocity km/s sigExt Standard deviation (external error) of the individual radial velocity observations km/s sigInt Expected average (internal) error of a single radial velocity as computed by XCSAO km/s sigExt/sigInt Ratio of external to internal errors --- chi2 Chi-square of the data set for this star --- P(chi2) Probability that chi^2 is due to observational errors of a true constant-velocity object % <R> Average goodness-of-fit parameter R, from XCSAO --- <height> Average correlation height, from XCSAO --- Mean radial velocities, luminosity ratios, and other derived parameters for 65 stars with double-lined or composite spectra HD HD number of double-lined star --- m_HD Visual binary component code --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Teff1 Synthetic template spectrum effective temperature, for component 1 in spectrum K Vrot1 Synthetic template spectrum rotational velocity, for component 1 in spectrum km/s Teff2 Synthetic template spectrum effective temperature, for component 2 in spectrum K Vrot2 Synthetic template spectrum rotational velocity, for component 2 in spectrum km/s Alpha Luminosity ratio (comp2/comp1) computed with TODCOR (see text) --- Nobs Number of observations --- <V0> Mean (systemic) radial velocity, V0 km/s e_<V0> Mean error of mean radial velocity km/s Span Time span from first to last observation d q Mass ratio q (comp2/comp1) when available; see paper for methods of computation --- e_q Mean error of mass ratio --- Rem Remark on nature of system number=1 SB2/3 indicates no. of components detected; O: preliminary single- or double-lined orbit computed (see Table 3 and Figure 2); W: V0 and q computed by Wilson's (1941ApJ....93...29W) method; C: velocities constant during period of observation --- List of stars which rotate too rapidly for usable radial-velocity measurements with the CfA instruments HD HD number, for fast-rotating stars not measurable with the current CfA instruments --- m_HD Visual binary component code --- Individual radial-velocity observations for the single-lined stars HD HD number, as in table1 --- m_HD Visual binary component code --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Tel Observatory code number=1 "W": 1.5m Wyeth; "T": 1.5m Tillinghast; "M": MMT 4.2m telescope --- Obs Serial number of observation --- Star Associated star identification to serial number of observation --- log[Fe/H] Metal abundance (always solar = 00 here) [Sun] Teff Effective temperature (Template spectrum parameter) K logg Surface gravity (Template spectrum parameter) [mm/s2] Vrot Value of vsini selected for the star (Template spectrum parameter) km/s HJD Heliocentric Julian Date of observation d RV Radial velocity km/s e_RV Mean error of radial velocity as computed by XCSAO km/s R Goodness-of-fit parameter R, from XCSAO ---- height Correlation peak height, from XCSAO --- Individual radial-velocity observations for the double-lined stars HD HD number, as in table2 --- m_HD Visual binary component code --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Teff1 Synthetic template spectrum effective temperature for component 1 in spectrum K Vrot1 Synthetic template spectrum rotational velocity for component 1 in spectrum km/s Teff2 Synthetic template spectrum effective temperature for component 2 in spectrum K Vrot2 Synthetic template spectrum rotational velocity for component 1 in spectrum km/s Alpha Continuum ratio alpha (comp2/comp1) specified to TODCOR when fixed for all observations --- n_Alpha f if continuum ratio alpha (comp2/comp1) was determined by TODCOR for each observation --- HJD Heliocentric Julian Date of observation d RV1 Radial velocity of component 1 km/s RV2 Radial velocity of component 2 km/s L2/L1 Luminosity ratio (comp2/comp1), see above --- height Correlation peak height, from TODCOR --- Obs Running number of observation --- Patricia Bauer CDS 1997 Jun 13 Johannes Andersen <ja@ursa.astro.ku.dk> J_A+AS_126_21.xml Penetrating the zone of avoidance. IV. An optical survey for galaxies in the region 130<l<180, -5<b<+5 J/A+AS/126/247 J/A+AS/126/247 Galaxies in the "zone of avoidance". IV. Penetrating the zone of avoidance. IV. An optical survey for galaxies in the region 130<l<180, -5<b<+5 W Saurer R Seeberger R Weinberger Astron. Astrophys. Suppl. Ser. 126 247 1997 1997A&AS..126..247S J/A+AS/110/269 : Part. I, |b| <= 5 (Weinberger+, 1995) J/A+AS/117/1 : Part II, 180<l<240 (Seeberger+, 1996) J/A+AS/117/369 : Part III, 120<l<130, |b|<10 (Lercher+, 1996) Cross identifications Galaxy catalogs catalogs dust, extinction galaxies: clusters: individual (Psc-Per supercluster) galaxies: general Galaxy: structure As the fourth part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1067 galaxies discovered during a systematic search on Palomar Observatory Sky Survey I (POSSI) red-sensitive prints. The region searched comprises 500 square degrees, at 130{deg}<=l<=180{deg}, -5{deg}<=b<=+5{deg}. In addition to galactic and equatorial coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints and made cross checks with the IRAS PSC catalogue. An asymmetric distribution of the galaxies with respect to the galactic equator is found and is compared to the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. There is a pronounced bridge of galaxies across the galactic plane at l=~160{deg} which will be discussed according to recent results on the extension of the Pisces-Perseus supercluster.
Optically detected galaxies in the region 130 < l < 180, |b| < 5 Name Zone Of Avoidance Galaxy Name of the galaxy in galactic coordinate --- RAh1950 Right ascension B1950 h RAm1950 Right ascension B1950 min RAs1950 Right ascension B1950 s DE-1950 Declination sign --- DEd1950 Declination B1950 deg DEm1950 Declination B1950 arcmin RAh2000 Right ascension J2000 h RAm2000 Right ascension J2000 min RAs2000 Right ascension J2000 s DE-2000 Declination sign --- DEd2000 Declination J2000 deg DEm2000 Declination J2000 arcmin POSS POSS print --- xpos Cartesian x-coordinate on POSS mm ypos Cartesian y-coordinate on POSS mm DmajE Maximum diameter on POSS-E (red) arcmin DminE Minimum diameter on POSS-E (red) arcmin DmajEc Maximum diameter of the core on POSS-E (red) arcmin DmajO Maximum diameter on POSS-O (blue) arcmin DminO Minimum diameter on POSS-O (blue) arcmin DmajOc Maximum diameter of the core on POSS-O (blue) arcmin Ident Cross-identifications and remarks --- Patricia Bauer CDS 1997 Apr 11 Walter Saurer <walter@ast6.uibk.ac.at> J_A+AS_126_247.xml An Atlas of high resolution synthetic spectra in the wavelength region 4850-5400 A J/A+AS/126/267 J/A+AS/126/267 Atlas of Synthetic Spectra An Atlas of high resolution synthetic spectra in the wavelength region 4850-5400 A M Chavez M L Malagnini C Morossi Astron. Astrophys. Suppl. Ser. 126 267 1997 1997A&AS..126..267C Spectroscopy Stars, late-type stars: atmospheres stars: late-type A library of 711 cool star synthetic spectra is presented. The coverage in the parameter space span in surface gravity from 1.0 to 5.0dex at a step of 0.5dex. The range in effective temperature covers from 4000 to 6000K at a step of 250K plus the spectra for 7000 and 8000K. The global chemical compositions are [M/H]=-1.0, -0.5, 0.0, +0.1, +0.2, +0.3 and +0.5. The adopted value of microturbulent velocity is 2km/s but for two sets of nine spectra each. All the spectra are computed at a resolving power =250,000. For each wavelength point the continuum and line blanketed absolute fluxes per unit frequency are given.
Summary of spectra File Filename (in subdirectory dat) --- Teff Effective temperature K logg Surface gravity [cm/s] [M/H] Metallicity --- Vtur Turbulant velocity km/s L/H Microturbulent parameter --- RP Resolving power --- Patricia Bauer CDS 1997 Oct 02 Maria Lucia Malagnini <malagnini@astrts.oat.ts.astro.it> J_A+AS_126_267.xml The solar disk spectrum between 660 and 1175 A. (First Order) obtained by SUMER on SOHO J/A+AS/126/281 J/A+AS/126/281 Solar disk spectrum The solar disk spectrum between 660 and 1175 A. (First Order) obtained by SUMER on SOHO W Curdt U Feldman J M Laming K Wilhelm U Schuehle P Lemaire Astron. Astrophys. Suppl. Ser. 126 281 1997 1997A&AS..126..281C Spectra, ultraviolet Sun Sun: chromosphere Sun: atmosphere transition region ultraviolet: general The near-limb quiet-Sun spectrum recorded on January 25, 1996 near the solar North pole is presented in tabular form and in graphical form. Table 1 - the line list - lists all lines found in the spectrum providing absolute peak intensities, measured and literature wavelengths, identification, and classification of the transition. Fig. 4 is a display the composite spectrum. The most prominent lines are labelled. In this figure intensities are given in instrumental units and logarithmic scale.
SOHO
*Line list Peak Peak intensity number=1 The continuum background is not subtracted. These entries have been corrected for the instrument spectral response by applying the radiometric calibration. Intensities of EUV lines in the upper solar atmosphere changes on short time scales. Since the various parts of the spectrum were not recorded simultaneously, the numbers in the first column should be used only as rough indications to the relative strengths of the particular transition. Blends normally have no intensity (or wavelength measurement entry) except for some cases where they could partially be separated. The same applies for members of the Lyman series since their line shape is strongly affected by the self-absorption. Blends are indicated in bl column. 10mW/m2/sr/nm n_Peak Note on peak --- lambda wavelength (literature) number=2 Wavelengths are mostly from the compilation by R.L. Kelly (1987, J. Phys. Chem. Ref. Data 16, 1). For lines with blends more than one wavelength is given, including unresolved lines if there is evidence (e.g. from the second order spectrum) that they may contribute to some extent. 0.1nm lambdaObs wavelength as observed number=3 The wavelengths were obtained by averaging measurements from two different detector recordings. Lines without identification are included as well and indicated by a '?' 0.1nm n_lambdaObs Note number=4 *: Lines taken as reference lines for the wavelength calibration. --- Ion Ion or atom --- Transu Transition, upper level --- --- dash --- Transl Transition, lower level --- bl Blend number=5 p: blended with preceding line n: blended with next line --- Rem Remarks number=6 Questionable identifications are marked by a '?' --- table1.tex LaTeX version of table1 fig4.ps *Composite spectrum The most prominent lines are labelled. In this figure intensities are given in instrumental units and logarithmic scale. Patricia Bauer CDS 1997 Apr 24 Werner Curdt <CURDT@linsu1.mpae.gwdg.de> J_A+AS_126_281.xml Abundances in planetary nebulae near the galactic centre. I. Abundance determinations J/A+AS/126/297 J/A+AS/126/297 PN abundances Abundances in planetary nebulae near the galactic centre. I. Abundance determinations M A Ratag S R Pottach M Dennefeld J Menzies Astron. Astrophys. Suppl. Ser. 126 297 1997 1997A&AS..126..297R V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) Abundances Planetary nebulae Galaxy: center ISM: abundances planetary nebulae: general Abundance determinations of about 110 planetary nebulae, which are likely to be in the Galactic Bulge are presented. Plasma diagnostics have been performed by making use of the available forbidden line ratios combined with radio continuum measurements. Chemical abundances of He, O, N, Ne, S, Ar, and Cl are then derived by employing theoretical nebular models as interpolation devices in establishing the ionization correction factors (ICFs) used to estimate the distribution of atoms among unobserved ionization stages. The overall agreement between the results derived by using the model-ICFs and those obtained from the theoretical models is reasonably good. The uncertainties related to the total abundances show a clear dependence on the level of excitation. In most cases, the abundances of chlorine can be derived only in objects with a relatively high Cl-abundance. Contrary to the conclusion previously drawn by Webster (1988MNRAS.230..377W), we found the excitation classes are not uniformly distributed. A clear peak at about classes 5 and 6 is noticed. The distribution is shifted toward a lower excitation range with respect to that of the nearby nebulae, reflecting the difference in the central star temperature distribution between the two samples.
Planetary nebulae J2000 positions PK PK name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Name PK name in Simbad --- Line Intensities corrected for interstellar extinction PN Planetary nebula name --- Lambda Wavelength --- Ident Wavelength identification --- l_Int Limit lfag on Int --- Int Line intensity number=2 Additional and adopted line intensities: Line intensities of the wavelengths marked with "w" are adopted from Webster (1988MNRAS.230..377W), while those with "a" from Aller and Keyes (1987ApJS...65..405A). 0-2.3 5007w, 5755w 0+3.1 4712w, 4740w 1-3.1 5007w, 6300w, 5698=1.04 2-6.1 6300a 2-4.2 4648=3.8, 5150=0.53, 5412=1.68, 5665+5680=2.6, 7236=1.36 ([ArIV], CII) 2-4.1 9069=18.0, 9532=48.0 2-3.5 3868a, 4471a 2-3.3 4415=1.1; 4553=1.52; 4570=1.62; 4681=3.9, 5698=2.8; Central star is probably a Wolf-Rayet. 2-2.4 5517a, 5537a 3-4.9 5412=2.2, 7236=1.1 ([ArIV],CII) 3-4.4 4648=3.8, 5412=4.2 4-22.1 Sum 4640-4648=7.4 6+4.2 5810=28.6 (broad) 6+8.1 4570=0.74; 7236=0.26 ([ArIV],CII) 7-4.1 3727a, 3968a, 5698=1.65 12-2.1 5698=1.37 349+4.1 4415=5.6 351+5.1 7236=0.77: ([ArIVl,CII) 353+6.2 6300a 355-6.1 5412=0.52 355-4.2 5517w, 5537w, 7236=0.7: ([ArIV],CII) 355-2.3 3425=87.1. Peculiar, if this is originated from [NeV], since no HeII line is detected. 357-7.1 4640w, 4686w 358+1.1 4686w, 4712w, 5755w 359-4.2 3425=251 (see remarks for PK 355-2.3) 359-2.3 5412=1.37 359-1.2 5876w 359-1.1 5412=3.1, 7012=1.70, sum (5517+5537)w 3-4.3 3727a, 4471a, 5876a, 6678a, 6717a, 6731a 3+3.1 5696=1.86: 4+6.2 7080=1.02 357+4.1 Sum (6717 +6731)w 359-2.4 4712w, 5200w, 6312w, 7325w 359+3.4 5412=7.8, 7005=6.0 --- u_Int Note number=1 ':' Uncertainty flag '?' Line not observed '*' Saturated line 'b' Blended with the preceding or next line --- Fundamental data of the newly observed objects Fundamental data of the objects with published spectra PK PK number --- Name Planetary nebula name --- Class Exc. class --- l_S6cm Limit flag on S6cm --- S6cm Flux density at 6cm mJy u_S6cm Uncertainty flag on S6cm --- logF(Hbeta) H{beta} flux [mW/m2] u_logF(Hbeta) Uncertainty flag on logF(Hbeta) --- l_Diam Limit flag on Diam --- Diam Diameter arcsec E(B-V)B Extinction E(B-V) from Balmer line mag E(B-V)r Extinction E(B-V) from radio/H{beta} mag u_E(B-V)r Uncertainty flag on E(B-V)r --- Te[OIII] Electron temperature from [OIII] 10+4K Te[NII] Electron temperature from [NII] 10+4K u_Te[NII] Uncertainty flag on Te[NII] --- Te Average electron temperature 10+4K u_Te Uncertainty flag on Te --- Ne Electron density 10+3cm-3 Vlsr LSR velocity km/s Fl/F(Hbeta) F_lambda_(5325A)/F(H{beta}) ratio 10+7m-1 FIR Total IR flux 10-13W/m2 IRE IR excess --- Ref References number=1 A: Acker et al. (1989A&AS...80..201A) A2: Acker et al. (1989A&AS...77..487A) AK: Aaquist and Kwok (1990A&AS...84..229A) AK1: Aller and Keyes (1987ApJS...65..405A) AL: Allen (1979Obs....99...83A) G: Gathier et al. (1983A&A...128..325G) KFL: Kinman et al. (1988AJ.....95..804K) MA: Milne and Aller (1975A&A....38..183M, 1982A&AS...50..209M) P: Pottasch et al. (1988A&A...205..248P) PK: Perek and Kohoutek (1967PKCat.C......1P) R: Ratag et al. (1990A&A...233..181R) S: Schneider et al. (1983ApJS...52..399S) SK: Shaw and Kaler (1989ApJS...69..495S) W: Webster (1988MNRAS.230..377W) W83: Webster (1983PASP...95..610W) Z: Zilstra et al. (1989IAUS..131..210Z) --- Adopted abundances for the nebulae Abundances from the literature PK PK name --- Name Other name --- [He] Adopted He abundance [Sun] n_[He] Note on [He] --- [O] Adopted O abundance [Sun] n_[O] Note on [O] --- [N] Adopted N abundance [Sun] n_[N] Note on [N] --- [Ne] Adopted Ne abundance [Sun] n_[Ne] Note on [Ne] --- [S] Adopted S abundance [Sun] n_[S] Note on [S] --- [Ar] Adopted Ar abundance [Sun] n_[Ar] Note on [Ar] --- u_[Ar] Uncertainty flag on [Ar] --- [Cl] Adopted Cl abundance [Sun] n_[Cl] Note on [Cl] --- Teff Effective temperature 10+3K logg Surface gravity [cm/s2] Notes Notes number=1 (1) Kurucz (1979ApJS...40....1K) (2) Clegg and Middlemass (1987MNRAS.228..759C) (3) Husfeld et al. (1984A&A...134..139H) (4) Planckian distribution. (5) The derived electron temperature, Te, is uncertain. (6) The electron density, Ne is derived from [ArIV] doublet. (7) The adopted electron density is uncertain. (8) The faintness, due to the very large interstellar extinction and/or due to the intrinsically low surface brightness of the nebula, causes the line intensities blueward of H{beta} to be poorly determined. (9) The observed line intensity ratio of [OII]{lambda}3727/{lambda}3725 cannot be reproduced by the model. The line intensity at {lambda}7325 predicted by the model is much lower than the observed one. Dielectronic recombination may play an important role (Rubin, 1986ApJ...309..334R). --- Patricia Bauer CDS 1997 Oct 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_126_297.xml UBVRI photometry of the FK5 Extension Catalogue Stars. J/A+AS/126/311 J/A+AS/126/311 UBVRI photometry of FK5 Ext. stars UBVRI photometry of the FK5 Extension Catalogue Stars. G Carrasco C Ledoux P Loyola Astron. Astrophys. Suppl. Ser. 126 311 1997 1997A&AS..126..311C I/149 : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) - Extension (Fricke+ 1991) Photometry, UBVRI Stars, fundamental catalogs techniques: photometric Table 1 includes: the star number in the E-regions; the HD or CPD number; the V magnitude; the B-V, U-V, V-R and R-I color indices; e, the mean square error of the averages published (unit: 0.001 magnitude); n, the number of observations for each star; and Sp, the spectral types (Graham, 1982PASP...94..244G). Table 2 gives similar information for the program stars. An asterisk after the star number means that the observations were made with a diaphragm, and a v means a variable star. The results of the observations of the FK5 Extension stars Nx 4173, 4409, 5355, 5400, 5410, 5593, 5671, 5886 and 6056 shows that they are variable stars; the published results correspond to the mean values obtained from the observations.
UBVRI photometry of the standard stars Name Star number in the E-regions --- n_Name *: Observations were made with a diaphragm --- HD/CPD HD (Cat. <III/135>) or CPD (Cat. <I/108>) number --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag 10-3mag B-V B-V colour index mag e_B-V rms uncertainty on B-V 10-3mag U-B U-B colour index mag e_U-B rms uncertainty on U-B 10-3mag V-R V-R colour index mag e_V-R rms uncertainty on V-R 10-3mag R-I R-I colour index mag e_R-I rms uncertainty on R-I 10-3mag Nobs Number of observations for each star --- SpType Spectral types (Graham 1982) --- UBVRI photometry of the program stars FK5 FK5 (Cat. <I/175>) number --- n_FK5 *: Observations were made with a diaphragm --- BD BD (Cat. <I/122>) name --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag 10-3mag B-V B-V colour index mag e_B-V rms uncertainty on B-V 10-3mag U-B U-B colour index mag e_U-B rms uncertainty on U-B 10-3mag V-R V-R colour index mag e_V-R rms uncertainty on V-R 10-3mag R-I R-I colour index mag e_R-I rms uncertainty on R-I 10-3mag Nobs Number of observations for each star --- SpType Spectral types (Graham 1982) --- Var v: variable star --- Patricia Bauer CDS 1997 Sep 26 Patricio Loyola <ployola@das.uchile.cl> J_A+AS_126_311.xml A Catalogue of Compact Radio Sources in and behind the Large Magellanic Cloud J/A+AS/126/325 J/A+AS/126/325 Compact Radio Sources in & behind LMC catalogue A Catalogue of Compact Radio Sources in and behind the Large Magellanic Cloud M Marx J M Dickey U Mebold Astron. Astrophys. Suppl. Ser. 126 325 1997 1997A&AS..126..325M J/A+AS/111/31 : Radio continuum study of the MC (Filipovic+, 1995) J/A+AS/120/77 : Radio continuum study of the MC (Filipovic+, 1996) VIII/38 : The Parkes-MIT-NRAO 4.85GHz (PMN) Surveys (Griffith+ 1993-1996) Magellanic Clouds Radio sources HII regions Magellanic Clouds methods: statistical radio continuum: galaxies surveys We present the results of a continuum snapshot survey of a 3x4{deg}^2^ region of the Large Magellanic Cloud including the area of the giant molecular cloud and the 30 Doradus nebula. The observations have been carried out with the Australia Telescope Compact Array (ATCA) at 1.4 and 2.4GHz. Most fields are complete to about 6mJy peak flux density at 1.4GHz and to about 3mJy at 2.4GHz. The positions, peak and integral flux densities of 113 compact (<54") sources detected at 1.4GHz and of 70 sources (<34") detected at 2.4GHz are presented. Positions are accurate to about 3" and peak flux densities are accurate to about 10% or better, depending on the source position relative to the pointing centers. 32 of the sources detected at 1.4GHz are coincident with H{alpha} objects in the catalogue of Davies, Elliot and Meaburn (1976MmRAS..81...89D); these are possibly intrinsic to the LMC. However, we suppose that most are background objects, since the number vs. flux agrees with predictions of extragalactic source counts from other surveys.
The source list at 1.4 GHz The source list at 2.4 GHz Name Source name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Si Integrated flux density mJy Sp Peak flux density mJy l_uvr Limit flag on uvr --- uvr Spacing used number=1 Spacings used and values of the tapering when imaging the data with the AIPS routine MX, which combines the Fourier Transform imaging with the deconvolution of the synthesized beam. The results were obtained by restricting the data to baselines longer than 3k{lambda} to exclude the poorly sampled extended emission. --- uvt Value of the tapering number=1 Spacings used and values of the tapering when imaging the data with the AIPS routine MX, which combines the Fourier Transform imaging with the deconvolution of the synthesized beam. The results were obtained by restricting the data to baselines longer than 3k{lambda} to exclude the poorly sampled extended emission. --- Field Field in which the source was detected --- alpha Spectral index between 1.4 and 2.4GHz (only table4) --- Ident Identifications (only table3) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Apr 14 J_A+AS_126_325.xml Photometrically determined membership of the young, open cluster IC 2391 J/A+AS/126/357 J/A+AS/126/357 Members of IC 2391 Photometrically determined membership of the young, open cluster IC 2391 W R J Rolleston P B Byrne Astron. Astrophys. Suppl. Ser. 126 357 1997 1997A&AS..126..357R Clusters, open Photometry, CCD open clusters and associations: individual (IC 2391) stars: evolution stars: late-type New 4-colour BV(RI)_KC_ CCD photometry to a limiting magnitude of V=~19 is presented for 1428 objects observed towards the direction of the young, open cluster IC 2391. We observed 36 (2'x3') fields within 17arcmin of the nominal cluster core. By fitting the theoretical isochrones of D'Antona & Mazzitelli (1994ApJS...90..467D) to a combination of colour-magnitude and colour-colour diagrams, we have identified 17 stars as probable cluster members with a further 85 stars as possible members. The brightness distribution of low-mass members is compared with the luminosity function observed for the Pleiades and we estimate that the contamination due to background giants should be small.
IC 2391 08 40.2 -53 04
fig4.ps Identification charts for the candidate members of IC 2391 Patricia Bauer CDS 1997 Jul 08 R. Rolleston <R.Rolleston@Queens-Belfast.AC.UK> J_A+AS_126_357.xml Atomic data from the Iron Project. XXVII. Electron impact excitation collision strengths and rate coefficients for Fe IV J/A+AS/126/373 J/A+AS/126/373 IRON Project XXVII. Fe IV collision strengths Atomic data from the Iron Project. XXVII. Electron impact excitation collision strengths and rate coefficients for Fe IV H L Zhang A K Pradhan Astron. Astrophys. Suppl. Ser. 126 373 1997 1997A&AS..126..373Z J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions J/A+AS/123/159 : IRON Project XXII. C and O radiative rates J/A+AS/123/575 : IRON Project XXIII. Fe XXII excitation rate coefficients 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths 1997A&AS..122..167B : IRON Project XX. Fe I oscillator strengths 1997A&AS..122..177P : IRON Project XXI. Fe I fine-structure transition 1997A&AS..126..105B : IRON Project XXIV. Fe XXIV electron excitation 1997A&AS..126..365B : IRON Project XXVI. Fe IV oscillator strengths Atomic physics atomic processes HII regions planetary nebulae: general Collision strengths and maxwellian-averaged rate coefficients have been calculated for 8771 non-vanishing transitions among 140 fine structure levels, dominated by the configurations 3d^5^, 3d^4^4s, and 3d^4^4p in Fe IV. Collision strengths are calculated using the R-matrix method with a 49 term close-coupling target expansion for electron energies up to 15 rydbergs. Rate coefficients are tabulated for a wide range of temperatures in which Fe IV is abundant in plasma sources. A brief discussion of the calculations and sample results are given. The present rates for Fe IV are expected to find applications in spectral diagnostics of a variety of astrophysical sources.
Levels for table3 Index Level index --- Conf Electronic configuration --- Term Electronic term --- J Total angular momentum --- E Theoretical energy Ry Patricia Bauer CDS 1997 Sep 12 Honglin Zhang <zhang@astronomy.ohio-state.edu> J_A+AS_126_373.xml Hydrodynamical models and synthetic spectra of circumstellar dust shells around AGB stars. I. Stationary solutions. J/A+AS/126/39 J/A+AS/126/39 Models of circumstellar dust shells Hydrodynamical models and synthetic spectra of circumstellar dust shells around AGB stars. I. Stationary solutions. M Steffen R Szczerba A Men'shchikov D Schoenberner Astron. Astrophys. Suppl. Ser. 126 39 1997 1997A&AS..126...39S Models, evolutionary circumstellar matter dust, extinction hydrodynamics radiative transfer stars: AGB and post-AGB stars: mass-loss Main properties of the steady state hydrodynamical models of circumstellar gas/dust shells around late type giants, computed for different stellar parameters (mass, luminosity, effective temperature) and dust composition (astronomical silicates, graphite, or amorphous carbon, with properties given in Tab.1 and Fig.1). Each table lists the results as a function of the adopted mass loss rate for fixed stellar parameters and dust properties. Tables 2 - 11 are related to Figures 2 - 11: Each of the figures shows the velocity structure and the resulting spectral energy distribution for a subset of models listed in the respective table.
Models results (table2-11) Model Model name number=1 the models are: C1 to C6 models: M= 1, L=1E4, Teff=3000, Astr. silicates, u1=2 km/s (Table2) D1 to D5 models: M= 4, L=5E4, Teff=2500, Astr. silicates, u1=2 km/s (Table3) E1 to E5 models: M=10, L=4E5, Teff=2500, Astr. silicates, u1=4 km/s (Table4) F1 to F4 models: M=30, L=1E4, Teff=2500, Astr. silicates, u1=4 km/s (Table5) G1 to G6 models: M= 1, L=1E4, Teff=2000, Graphite, u1=2 km/s (Table6) H1 to H6 models: M= 3, L=5E4, Teff=2000, Graphite, u1=2 km/s (Table7) I1 to I5 models: M= 5, L=5E4, Teff=2000, Graphite, u1=2 km/s (Table8) J1 to J6 models: M= 1, L=1E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table9) K1 to K6 models: M= 3, L=5E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table10) L1 to L5 models: M= 5, L=5E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table11) Where M is Mstar (M_{sun}_), L is Lstar (L_{sun}_) , and u1 is the initial velocity (gas and dust) at the inner boundary r1. --- n_Model Note on Model number=2 For each mass loss rate, the second row (n_Model = n) lists the corresponding results from a model calculation ignoring gas pressure. Missing data indicate that no steady state solution was found. --- MassLoss Mass loss rate solMass/yr r1 Dust condensation radius 10+14cm l_r1/r* Limit flag on r1/r* --- r1/r* r1 in stellar radii --- l_ue Limit flag on ue --- ue Terminal gas outflow velocity km/s ue/vesc(r1) ue in units of escape velocity at r1 --- (w-u)/ue Terminal drift velocity in units of ue --- l_tauV Limit flag on tauV --- tauV Total optical depth at lambda 0.55 mum --- tau10 Total optical depth at lambda 10 mum --- tauF Flux-averaged total optical depth (Eq.25) --- Beta MassLoss*ue*c/L number=3 Beta = Mdot*ue*c/L = Ratio of momentum flux in the outflow to stellar photon momentum flux --- tables.tex LaTeX version of the tables Matthias Steffen Ast. Inst. Potsdam Patricia Bauer CDS 1997 Feb 26 Matthias Steffen <supas048@astrophysik.uni-kiel.de> J_A+AS_126_39.xml CO and HI in a southern sample of interacting galaxies. I. The data J/A+AS/126/3 J/A+AS/126/3 CO and HI in interacting galaxies CO and HI in a southern sample of interacting galaxies. I. The data C Horellou R S Booth Astron. Astrophys. Suppl. Ser. 126 3 1997 1997A&AS..126....3H Carbon monoxide Galaxies, H I data Radio lines galaxies: evolution galaxies: interactions galaxies: ISM radio lines: galaxies Using SEST, the Parkes antenna and the Australia Telescope Compact Array, we have made a survey of the ^12^CO(1-0) and HI emission of an optically-selected sample of =~60 southern interacting and merging galaxies. In this paper we present the data and determine global masses of neutral gas (in molecular and atomic form) for the observed galaxies. We have detected HI in 26 systems and found that these galaxies have less than 15% of their gas in molecular form.
Galaxy Characteristics Name Source name --- Note Note about individual galaxies number=1 a : JB01 has an uncertainty in position of 30x30arcsec. NED gives also a radio velocity of 10079km/s b : JB06_2 has an uncertainty in position of 30x30arcsec c : JB14_2 other authors give Vhel=6321km/s d : JB29_1 has an uncertainty in position of 30x30arcsec e : JB33 has an uncertainty in position of 9x9arcsec f : JB40 has an uncertainty in position of 5x5arcsec g : JB56 HI line at Vhel=2600km/s towards JB56 --- FileName Name of postscript figure file containing this galaxy (in this directory) --- Galaxy Galaxy name (from ESO survey) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Vhel Heliocentric velocity km/s MType Morphological Type --- logD25 Diameter at 25mag/arcsec2 (log scale) [0.1arcmin] OtherName Other designation of the Galaxy --- HI and CO observational results HIname Source name --- Note Note on source number=1 the notes are a = pointing made toward a position between galaxies JB11_1 and JB11_2 b = sources JB57 and JB58 observed together in HI d = sources not separated in HI, but are separated in CO n = not observed in HI --- posFlag Flag for uncertain (30x30") position --- vHI HI velocity km/s DvHI HI velocity width km/s l_SHI Limit flag on SHI --- SHI Integrated HI flux Jy.km/s e_SHI Mean error on HI flux Jy.km/s l_M(HI) Limit flag on M(HI) --- M(HI) Derived HI mass 10+9solMass Intrum Instrument used (Parkes or Australian Telescope Compact Array) --- Name Source name, as in table1 --- Note(CO) 'n' if not observed --- vCO CO velocity, observed at SEST telescope at ESO-La Silla. km/s DvCO CO velocity width km/s l_SCO Limit flag on SCO --- SCO Integrated antenna temperature K.km/s e_SCO Mean error on SCO K.km/s l_M(H2) Limit flag on M(H2) ('*' stands for tentative value) --- M(H2) Mass of H2 derived from CO data. 10+8solMass fig3p1.ps Optical images, HI and CO spectra fig3p2.ps Figure 3 continued fig3p3.ps Figure 3 continued fig3p4.ps Figure 3 continued fig3p5.ps Figure 3 continued fig3p6.ps Figure 3 continued fig3p7.ps Figure 3 continued fig3p8.ps Figure 3 continued fig3p9.ps Figure 3 continued fig3p10.ps Figure 3 continued fig3p11.ps Figure 3 continued fig3p12.ps Figure 3 continued Patricia Bauer CDS 1997 May 02 J_A+AS_126_3.xml Cepheids as tracers of star formation in M 31. I. Observations and identifications. J/A+AS/126/401 J/A+AS/126/401 M 31 Cepheids periods Cepheids as tracers of star formation in M 31. I. Observations and identifications. E A Magnier T Augusteijn S Prins J van Paradijs W H G Lewin Astron. Astrophys. Suppl. Ser. 126 401 1997 1997A&AS..126..401M Magnitudes Stars, variable Cepheids distance scale galaxies: individual (M 31) galaxies: stellar content stars: formation Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (<3%). For V<21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.
New M31 Cepheid Candidate Identifications ID Identification number --- RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Vmag Maximum V magnitude mag e_Vmag rms uncertainty on Vmag mag Per Period d e_Per rms uncertainty on Per d figure5.ps *Light curves of New Cepheid Candidates All 6 figures show the V lightcurves of the candidate Cepheids. A pair of dashed lines show the 1 sigma range of V (max). figure6.ps Light curves of New Cepheid Candidates figure7.ps Light curves of New Cepheid Candidates figure8.ps Light curves of New Cepheid Candidates figure9.ps Light curves of New Cepheid Candidates figure10.ps Light curves of New Cepheid Candidates Patricia Bauer CDS 1997 Sep 15 Eugene Magnier <gene@pikake.astro.washington.edu> J_A+AS_126_401.xml The Effelsberg 21cm radio continuum survey of the Galactic Plane between l=95.5 degree and l=240 degree J/A+AS/126/413 J/A+AS/126/413 21cm radio continuum survey. II. The Effelsberg 21cm radio continuum survey of the Galactic Plane between l=95.5 degree and l=240 degree P Reich W Reich E Fuerst Astron. Astrophys. Suppl. Ser. 126 413 1997 1997A&AS..126..413R J/A+AS/83/539 : 21cm radio continuum survey. I. (Reich+ 1990) Radio sources catalogs Galaxy: general surveys We analysed the 21cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 1830 radio sources with a maximum apparent size of 16' and peak flux densities >160mK or >79mJy/beam area, and a list of 884 radio sources with a maximum apparent size of 16' and peak flux densities >200mK or >98mJy/beam area.
List of 1830 small diameter radio sources No Source number --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec RA2000d Right ascension (J2000.0) h RA2000m Right ascension (J2000.0) min RA2000s Right ascension (J2000.0) s DE2000- Declination sign --- DE2000d Declination (J2000.0) deg DE2000m Declination (J2000.0) arcmin DE2000s Declination (J2000.0) arcsec Sint Integrated flux density Jy SPeak Peak flux density mJy MajAxis Major axis of gaussian arcmin --- --- MinAxis Minor axis of gaussian arcmin --- --- PA Galactic position angle of the ellipsoid deg Size Point-like sources or slightly extended sources number=1 PL = point-like sources, major axis x minor axis of gaussian <10x10arcmin^2^ SE = slightly extended sources, major axis x minor axis of gaussian <11x11arcmin^2^ --- e_Pos Positional error 10arcsec e_Sint Integrated flux density error 10% e_MajAxis Size error (on MajAxisand MinAxis) 20arcsec e_PA Error of the position angle 3deg Patricia Bauer CDS 1997 Sep 15 Patricia Reich <preich@mpifr-bonn.mpg.de> J_A+AS_126_413.xml Near infrared photometry of IRAS sources with colours like planetary nebulae. III. J/A+AS/126/479 J/A+AS/126/479 NIR photometry of IRAS sources. III Near infrared photometry of IRAS sources with colours like planetary nebulae. III. P Garcia-Lario A Manchado W Pych S R Pottasch Astron. Astrophys. Suppl. Ser. 126 479 1997 1997A&AS..126..479G Infrared sources Photometry, infrared infrared: general planetary nebulae: general stars: AGB and post-AGB We present the near infrared photometry of a new sample of 225 IRAS sources, many of them previously unidentified in the literature, selected because their far infrared colours are similar to those shown by known planetary nebulae. The results obtained are used to establish the main source of near infrared emission. Combining this information with the far infrared IRAS data and a few additional criteria we determine the nature and evolutionary stage of all the sources observed so far, including those for which near infrared photometry was previously reported in Papers I (Manchado et al., 1989A&A...214..139M) and II (Garcia-Lario et al., 1990A&AS...82..497G).
Observed magnitudes IRAS IRAS name --- m_IRAS Multiplicity index on IRAS --- l_Jmag Limit flag on Jmag --- Jmag J magnitude mag e_Jmag rms uncertainty on Jmag mag l_Hmag Limit flag on Hmag --- Hmag H magnitude mag e_Hmag rms uncertainty on Hmag mag Kmag K magnitude mag e_Kmag rms uncertainty on Kmag mag l_L'mag Limit flag on L'mag --- L'mag L' magnitude mag e_L'mag rms uncertainty on L'mag mag l_Mmag Limit flag on Mmag --- Mmag M magnitude mag e_Mmag rms uncertainty on Mmag mag Run Run number --- Other Other measurements number=1 References: 1: Paper I, Manchado et al. (1989A&A...214..139M) 2: Kenyon et al. (1990AJ.....99..869K) 3: Hrivnak & Kwok (1991ApJ...368..564H) 4: Paper II, Garcma-Lario et al. (1990A&AS...82..497G) 5: Kwok et al. (1995ApJ...454..394K) 6: Blommaert et al. (1993A&A...267...39B) 7: Allen (1974MNRAS.168....1A) 8: Allen (1973MNRAS.161..145A) 9: Hu et al. (1993A&AS..100..413H) 10: Campbell et al. (1989AJ.....98..643C) 11: Zijlstra et al. (1991A&A...243L...9Z) 12: Fouque et al. (1992A&AS...93..151F, Cat. <II/177>) 13: Kastner et al.(1992ApJ...398..552K) 14: Lepine et al. (1995, Cat. <J/A+A/199/453>) 15: Miroshnichenko et al. (1996A&A...312..521M) 16: Gaylard & Whitelock (1988MNRAS.235..123G) 17: Persson & Campbell (1988AJ.....96.1019P) 18: Liseau et al. (1992A&A...265..577L) 19: Allen & Glass (1975MNRAS.170..579A) 20: Hrivnak et al. (1989ApJ...346..265H) 21: Hu et al. (1990A&A...227L..17H) 22: Hu et al. (1989A&A...208..213H) 23: Gaylard et al. (1989MNRAS.236..247G) 24: Elias (1978ApJ...224..857E) 25: Lloyd-Evans (1985MNRAS.217..493L) 26: van der Veen et al. (1989A&A...226..108V) 27: Persi et al. (1987, in "Planetary and proto-planetary nebulae: from IRAS to ISO", Preite-Martinez A. (ed.). Reidel-Dordrecht, p. 221) 28: Le Bertre (1993, Cat. <J/A+AS/97/729>) 29: Epchtein et al. (1987A&AS...71...39E) 30: Nyman et al. (1993A&A...280..551N) 31: Epchtein & Nguyen-Q-Rieu (1982A&A...107..229E) 32: Hu et al. (1993A&A...273..185H) 33: Persi et al. (1990AJ.....99..303P) 34: Jones et al. (1982ApJ...253..208J) 35: Lawrence et al. (1990AJ.....99.1232L) 36: Hrivnak et al. (1988ApJ...331..832H) 37: Kastner & Weintraub (1995ApJ...452..833K) 38: Cohen (1974MNRAS.169..257C) 39: Whitelock et al. (1995MNRAS.276..219W) --- IRAS sources not detected in the K band IRAS IRAS name --- n_IRAS Note number=1 1: Detected in run (8) 2: The object detected in run (2) is 40" away from the IRAS position 3: Detected in run (6) 4: Detected in run (7) --- Run Run numbers --- Classification of individual sources Seq Sequence number in the sample --- NoteFlag Indicates a note in file notes.tex --- IRAS IRAS name --- Names Other names in the literature --- F12um IRAS flux density at 12 microns Jy [12]-[25] IRAS colour [12]-[25] --- [25]-[60] IRAS colour [25]-[60] --- LRS LRS class (see Cat. <III/197>) --- VAR IRAS variability index --- NIR Code from I to V indicating the position of the source in the NIR two-colour diagram --- CO CO detection code number=1 N = Not detected Y = Detected Y_n = Narrow Emission Detected Y? = Possible detection --- r_CO Reference for the CO detection number=3 References: 1: te Lintel Hekkert et al. (1991, Cat. <J/A+AS/90/327>) 2: David et al. (1993, Cat. <J/A+A/277/453>) 3: Ratag (1991, priv. comm.) 4: te Lintel Hekkert (1991A&A...248..209T) 5: Omont et al. (1993, Cat. <J/A+A/267/515>) 6: Wouterloot & Brand (1989, Cat. <J/A+AS/80/149>) 7: Likkel et al. (1991A&A...246..153L) 8: Wouterloot et al. (1993, Cat. <J/A+AS/98/589>) 9: Lewis (1992ApJ...396..251L) 10: Lewis et al. (1990ApJ...362..634L) 11: Woodsworth et al. (1990A&A...228..503W) 12: Casoli et al. (1986A&A...169..281C) 13: Nyman et al. (1992, Cat. <J/A+AS/93/121>) 14: Likkel (1989ApJ...344..350L) 15: Wouterloot et al. (1989A&A...215..131W) 16: Clemens & Barvainis (1988ApJS...68..257C) 17: Yun & Clemens (1994ApJS...92..145Y) 18: Hu et al. (1994A&AS..103..301H) 19: Davis et al. (1979ApJ...230..434D) 20: Garcia-Lario et al. (1993A&A...267L..11G) 21: Loup et al. (1990A&A...227L..29L) 22: Zijlstra et al. (1991A&A...243L...9Z) 23: Zuckerman et al. (1986ApJ...304..401Z) 24: Bujarrabal et al. (1992A&A...257..701B) 25: van der Veen et al. (1993A&A...269..231V) 26: de Vries et al. (1984A&AS...56..333D) 27: Knapp & Morris (1985ApJ...292..640K) 28: Knapp (1986ApJ...311..731K) 29: Morris et al. (1987ApJ...321..888M) 30: te Lintel Hekkert et al. (1989A&AS...78..399T) and references therein 31: te Lintel Hekkert et al. (1988A&A...202L..19T) 32: Hu et al. (1993A&AS..100..413H) 33: Silva et al. (1993A&A...275..510S) 34: Brand et al. (1987A&AS...68....1B) 35: Bujarrabal & Bachiller (1991A&A...242..247B) 36: Chapman (1988MNRAS.230..415C) 37: Gaylard et al. (1989MNRAS.236..247G) 38: Zijlstra et al. (1989A&A...217..157Z) 39: Sevenster et al. (1997b, submitted) 40: Likkel & Morris (1988ApJ...329..914L) 41: Zuckerman & Dyck (1986ApJ...311..345Z) 42: Sevenster et al. (1997, Cat. <J/A+AS/122/79>) 43: van Langevelde et al. (1992ApJ...396..686V) 44: Frail & Beasley (1994A&A...290..796F) 45: Slysh et al. (1994A&AS..106...87S) 46: Mauersberger et al. (1988A&A...206L..34M) 47: Knapp et al. (1995ApJ...455..293K) 48: Likkel et al. (1987A&A...173L..11L) 49: Zuckerman & Dyck (1989A&A...209..119Z) 50: Lewis et al. (1987AJ.....94.1025L) 51: Eder et al. (1988ApJS...66..183E) 52: Volk et al. (1993ApJ...402..292V) 53: Arquilla et al. (1986MNRAS.220..125A) 54: Knapp et al. (1989ApJ...336..822K) 55: Galt et al. (1989AJ.....98.2182G) 56: Zuckerman et al. (1977ApJ...211L..97Z) 57: Jenness et al. (1995MNRAS.276.1024J) 58: Lindqvist et al. (1988A&A...205L..15L) 59: Garcia-Lario et al. (1991A&A...249..223G) --- OH OH detection code number=2 N = Not detected Y = Double peak Y' = Absorption Y? = Possible detection Y_1 = Single peak Y_1?= Possible Single peak Y_m = Multiple peaks Y_1667_= Detected only at 1667 MHz --- r_OH Reference for the OH detection number=3 References: 1: te Lintel Hekkert et al. (1991, Cat. <J/A+AS/90/327>) 2: David et al. (1993, Cat. <J/A+A/277/453>) 3: Ratag (1991, priv. comm.) 4: te Lintel Hekkert (1991A&A...248..209T) 5: Omont et al. (1993, Cat. <J/A+A/267/515>) 6: Wouterloot & Brand (1989, Cat. <J/A+AS/80/149>) 7: Likkel et al. (1991A&A...246..153L) 8: Wouterloot et al. (1993, Cat. <J/A+AS/98/589>) 9: Lewis (1992ApJ...396..251L) 10: Lewis et al. (1990ApJ...362..634L) 11: Woodsworth et al. (1990A&A...228..503W) 12: Casoli et al. (1986A&A...169..281C) 13: Nyman et al. (1992, Cat. <J/A+AS/93/121>) 14: Likkel (1989ApJ...344..350L) 15: Wouterloot et al. (1989A&A...215..131W) 16: Clemens & Barvainis (1988ApJS...68..257C) 17: Yun & Clemens (1994ApJS...92..145Y) 18: Hu et al. (1994A&AS..103..301H) 19: Davis et al. (1979ApJ...230..434D) 20: Garcia-Lario et al. (1993A&A...267L..11G) 21: Loup et al. (1990A&A...227L..29L) 22: Zijlstra et al. (1991A&A...243L...9Z) 23: Zuckerman et al. (1986ApJ...304..401Z) 24: Bujarrabal et al. (1992A&A...257..701B) 25: van der Veen et al. (1993A&A...269..231V) 26: de Vries et al. (1984A&AS...56..333D) 27: Knapp & Morris (1985ApJ...292..640K) 28: Knapp (1986ApJ...311..731K) 29: Morris et al. (1987ApJ...321..888M) 30: te Lintel Hekkert et al. (1989A&AS...78..399T) and references therein 31: te Lintel Hekkert et al. (1988A&A...202L..19T) 32: Hu et al. (1993A&AS..100..413H) 33: Silva et al. (1993A&A...275..510S) 34: Brand et al. (1987A&AS...68....1B) 35: Bujarrabal & Bachiller (1991A&A...242..247B) 36: Chapman (1988MNRAS.230..415C) 37: Gaylard et al. (1989MNRAS.236..247G) 38: Zijlstra et al. (1989A&A...217..157Z) 39: Sevenster et al. (1997b, submitted) 40: Likkel & Morris (1988ApJ...329..914L) 41: Zuckerman & Dyck (1986ApJ...311..345Z) 42: Sevenster et al. (1997, Cat. <J/A+AS/122/79>) 43: van Langevelde et al. (1992ApJ...396..686V) 44: Frail & Beasley (1994A&A...290..796F) 45: Slysh et al. (1994A&AS..106...87S) 46: Mauersberger et al. (1988A&A...206L..34M) 47: Knapp et al. (1995ApJ...455..293K) 48: Likkel et al. (1987A&A...173L..11L) 49: Zuckerman & Dyck (1989A&A...209..119Z) 50: Lewis et al. (1987AJ.....94.1025L) 51: Eder et al. (1988ApJS...66..183E) 52: Volk et al. (1993ApJ...402..292V) 53: Arquilla et al. (1986MNRAS.220..125A) 54: Knapp et al. (1989ApJ...336..822K) 55: Galt et al. (1989AJ.....98.2182G) 56: Zuckerman et al. (1977ApJ...211L..97Z) 57: Jenness et al. (1995MNRAS.276.1024J) 58: Lindqvist et al. (1988A&A...205L..15L) 59: Garcia-Lario et al. (1991A&A...249..223G) --- Type Tentative classification --- table6.tex LaTeX version of table6 notes.tex LaTeX version of notes on individual objects tables.ps Postscript version of table6* + notes P. Garcia-Lario Leiden Observatory, NL Patricia Bauer CDS 1997 Apr 15 Pedro Garcia Lario <pgl@laeff.esa.es> J_A+AS_126_479.xml Scaleheights of 486 southern spiral galaxies and some statistical correlation J/A+AS/126/503 J/A+AS/126/503 Southern spiral galaxies scaleheights Scaleheights of 486 southern spiral galaxies and some statistical correlation J Ma Q Peng R Chen Z Ji C Tu Astron. Astrophys. Suppl. Ser. 126 503 1997 1997A&AS..126..503M Galaxies, optical Morphology galaxies: fundamental parameters galaxies: spiral galaxies: structure Based on Peng's method (1988A&A...206...18P), we obtain scaleheights of 486 southern spiral galaxies, the images of which are taken from the Digitized Sky Survey at Xinglong Station of Beijing Astronomical Observatory. The fitted spiral arms of 70 galaxies are compared with their images to get their optimum inclinations. The scaleheights of other 416 ones are listed in Table 1 in Appendix. After compiling and analyzing the data, we find some statistical correlations. The most interesting results are that a flatter galaxy is bluer and looks brighter, and galaxies become flatter along the Hubble sequence Sab-Scd.
*The Measuring and Fitting Results NGC NGC name many invalid NGC designations have been removed in May 1998 (see the "History" section below); the corrections have however NOT been performed on the latex version. --- PGC PGC name --- MType Mean revised morphological type --- gamma Optimum inclination of the galaxy gamma is defined by the equation gamma = arccos(d_25_/D_25_), where d_25_ and D_25_ are the minor and major isophotal diameters measured at or reduced to the surface brightness level mu_B_=25.0B-m/ss. deg Dist Distance of the galaxy from the Galactic Center Mpc H/D25 Flatness of the galaxy --- e_H/D25 rms uncertainty on H/D25 % h Apparent scaleheight of a galaxy arcmin e_h rms uncertainty on h % H Scaleheight of the galactic disk kpc e_H rms uncertainty on H % LAMDBA Wound parameter of a spiral arm --- e_LAMDBA rms uncertainty on LAMDBA % rho0 Angular diameter of the innermost point of the spiral arm from the Galactic Center arcmin SR Standard deviation discussed in Peng's paper (1988A&A...206...18P). --- tablea1.tex *LaTeX version of tablea1 Patricia Bauer, Francois Ochsenbein CDS 1998 May 09 Jun Ma <qhpeng@netra.nju.edu.cn> UNKNOWN UNKNOWN * 06-Jun-1997: LaTeX version received and archived at CDS from Jun Ma (qhpeng@netra.nju.edu.cn) * 09-May-1998: M. Schmitz (zb4ms@ipac.caltech.edu) communicated the problem of wrong NGC numbers in many entries of the table. The NGC designations were removed in entries for which the PGC (Cat. <VII/119>) does not list a NGC cross-identification; the latex version of the table was not modified. J_A+AS_126_503.xml Multiwavelength observations of the field HS 47.5/22 in Ursa Major. I. The X-ray catalogue of a medium deep ROSAT survey. J/A+AS/126/509 J/A+AS/126/509 HS 47.5/22: X-ray catalogue Multiwavelength observations of the field HS 47.5/22 in Ursa Major. I. The X-ray catalogue of a medium deep ROSAT survey. K Molthagen H J Wendker U G Briel Astron. Astrophys. Suppl. Ser. 126 509 1997 1997A&AS..126..509M IX/11 : ROSAT PSPC Source Catalog (Voges+ 1994) Magnitudes X-ray sources catalogs methods: data analysis surveys X-rays: galaxies X-rays: general Table 4 contains the parameters of the PSPC pointings which form the medium deep survey in HS 47.5/22, table 5 is the final X-ray source catalogue, and table 6 gives the results of the optical follow-up observations.
ROSAT
Parameters of the PSPC pointings which form the survey WG700 Pointing number; prefix WG700 --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin Texp Pointing exposure time s DATE Observation Date --- CRlim0 Limiting count rate at zero off axis angle 10-2ct/s CRlim40 Limiting count rate at 40' off axis angle 10-2ct/s X-ray source catalogue Seq Sequence number --- Name RXJ name (hhmm.m+dd'') --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Rad Identification search radius R = 2*sigma_pos+10" arcsec ML Likelihood --- CR Broad band count rate 10-2ct/s e_CR Count rate error 10-2ct/s FLAGS Flags number=1 I: detected in individual pointings M: detected in the merged data IM: detected in individual and merged data (RA, DE, ML from the former) MI: detected in individual and merged data (RA, DE, ML from the latter) 1: broad band detection 2: soft band detection 3: hard band detection 4: h1 band detection 5: h2 band detection --- Dist Distance between merged data and individual pointing detection arcsec NH Galactic HI column density 10+20cm-2 Bmag Apparent B magnitude mag e_Bmag B magnitude error mag IDENT Identification number=2 Object types: star: known stars D: visible on HQS direct plate only AGN: confirmed AGN st.can.: star-like on HQS plates (no further distinction possible) Abell 851: Abell cluster A851 gal.can.: galaxy candidate cl.can.: cluster candidate AGN can.: AGN candidate (including weak blue objects) empty: empty fields on the HQS direct plate FG/K/M can.: FG, K, or M star candidate sat.: saturated objective prism spectrum (mostly stars) unid.: unidentified object red: object with very weak and red objective prism spectrum gal.: galaxy ELG: emission line galaxy group: group of three active galaxies M st.: M star identified during this work Remarks: a: observed in this work b: Engels et al. 1997 (in prep.) c: Bade et al. 1995A&AS..110..469B, Cat. <J/A+AS/110/469> d: Puchnarewicz et al., 1992MNRAS.256..589P e: Notni, 1980AN....301...51N f: Klemola et al., 1987AJ.....94..501K, Cat. <I/199> and <I/200> g: Peterson et al., 1978PASP...90..386P h: chneider et al., 1994AJ....107.1245S, Cat. <J/AJ/107/1245> i: Schmidt et al., 1986ApJ...310..518S j: the source is located in the disk of galaxy UGC 5354, no B available k: another star with B=19.6+/-0.3 has been rejected as identification because of unrealistic log (fx/fb) --- Optical follow-up observations Seq Sequence number --- Name RXJ name --- Notes Footnotes number=1 a: B from objective prism plate b: previously identified in Bade et al. (1995, Cat. <J/A+AS/110/469>) c: observed with the Russian 6m telescope --- RAh Optical right ascension (J2000) h RAm Optical right ascension (J2000) min RAs Optical right ascension (J2000) s DEd Optical declination (J2000) deg DEm Optical declination (J2000) arcmin DEs Optical declination (J2000) arcsec Texp Exposure time (spectrum) s Bmag B magnitude mag e_Bmag B magnitude error mag z Redshift (if available) --- Ident Identification --- Patricia Bauer CDS 1997 Apr 24 Kerstin Molthagen <st2g303@hs.uni-hamburg.de> J_A+AS_126_509.xml Kinematical data on early-type galaxies. III. J/A+AS/126/519 J/A+AS/126/519 Kinematical data on early-type galaxies. III. Kinematical data on early-type galaxies. III. F Simien P Prugniel Astron. Astrophys. Suppl. Ser. 126 519 1997 1997A&AS..126..519S J/A+AS/122/521 : Kinematical data on early-type galaxies. I. (Simien+ 1997) J/A+AS/126/15 : Kinematical data on early-type galaxies. II. (Simien+ 1997) Galaxies, rotation Radial velocities Velocity dispersion galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: general galaxies: kinematics and dynamics We present new kinematical data for a sample of 24 early-type galaxies. Rotation curves and velocity-dispersion profiles are determined for 21 objects, while the central velocity dispersions are given for the whole sample. This is our third paper in a series devoted to the presentation of kinematical data on elliptical and S0 galaxies, derived from long-slit absorption spectroscopy.
Catalog elements for program galaxies Name Object identification number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) --- MType Morphological type number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) --- RAh Right Ascension 1950 (hours) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) h RAm Right Ascension 1950 (minutes) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) min RAs Right Ascension 1950 (seconds) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) s DE- Declination 1950 (sign) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) --- DEd Declination 1950 (degrees) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) deg DEm Declination 1950 (minutes) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) arcmin DEs Declination 1950 (seconds) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) arcsec RV Heliocentric radial velocity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) km/s BT Integrated blue magnitude number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) mag Dist Distance modulus number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) mag Re Effective radius number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) arcsec Eps Ellipticity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) --- PA Position angle of slit PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) deg r_Eps Reference for Eps and PA 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) --- Sig0 Central velocity dispersion number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) km/s e_Sig0 Error on Sig0 number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) km/s l_Vmax Upper-limit flag on Vmax number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) --- Vmax Maximum rotational velocity number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) km/s e_Vmax Error on Vmax number= PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). number= 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard (1985A&AS...59..205M) 3 = Michard & Marchal (1993A&AS...98...29M) 4 = LEDA (status: LEDA1996) km/s Log of the observations Name Object identification number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). --- Date Date of observation number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). "DD/MM/YY" PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). deg Nexp Number of exposures number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). --- Texp Exposure time number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). min Seeing Seeing FWHM number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). arcsec u_Seeing uncertainty flag on Seeing number= PA (North --> East) is in the range [0, 360[, and with a convention about the radius r in the profiles (see table 4). --- Kinematical results (mostly central values) Name Object identification --- Vhel Heliocentric radial velocity km/s u_Vhel uncertainty flag on Vhel --- e_Vhel Mean error on Vhel km/s sig0 Central velocity dispersion number=1 Rotation and dispersion velocities are projected along the line of sight km/s u_sig0 uncertainty flag on sig0 --- e_sig0 Mean error on sig0 km/s l_Vmax Upper-limit flag on Vmax --- Vmax Maximum rotational velocity number=1 Rotation and dispersion velocities are projected along the line of sight km/s u_Vmax uncertainty flag on Vmax --- e_Vmax Mean error on Vmax km/s rmax Radius corresponding to Vmax arcsec Profiles of velocity dispersion and rotation Name Object identification number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. --- PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg r Radius (<0 and >0 on opposite semi-axes) number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. arcsec Vrot Projected mean stellar rotation velocity Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s e_Vrot Mean error on Vrot number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s sigma Projected velocity dispersion number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s e_sigma Mean error on sigma number= Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. number= PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s Francois Simien, Patricia Bauer CDS 1997 Nov 25 Francois Simien <fs@cumulus.univ-lyon1.fr> J_A+AS_126_519.xml Morphological classification and structural parameter of galaxies in the Coma and Perseus clusters J/A+AS/126/67 J/A+AS/126/67 Coma and Perseus clusters galaxies Morphological classification and structural parameter of galaxies in the Coma and Perseus clusters S Andreon E Davoust P Poulain Astron. Astrophys. Suppl. Ser. 126 67 1997 1997A&AS..126...67A J/A+AS/116/429 : Classification of Coma early galaxies. (Andreon+ 1996) (Paper I) Galaxy catalogs Morphology Photometry, surface galaxies: clusters: individual (Coma, Abell 1656) galaxies: elliptical and lenticular, cD galaxies: fundamental parameters individual: (Perseus, Abell 426) We present the results of an isophotal shape analysis of galaxies in the Coma and Perseus clusters. These data, together with those of two previous papers, provide two complete samples of galaxies with reliable Hubble types in rich clusters: 1) all galaxies brighter than m_b_=16.5 falling within one degree (=2.3Mpc) from the center of the Coma cluster (187 galaxies), 2) all galaxies brighter than m_(Zwicky)=15.7 in a region of 5 deg 3' times 5 deg 27' around the center of the Perseus cluster (139 galaxies). These two complete samples cover 5 orders of magnitude in galaxy density and span areas of 91 and 17Mpc^2^, clustercentric radii up to 2.3 and 6.4Mpc, for Perseus and Coma respectively. They will be used in subsequent papers to study the dependence of galaxy types on cluster environment and as reference samples in comparisons with distant clusters.
Observing log of Perseus galaxies Name Name --- Run Observing run number=1 feb93: CCD Thompson 1024x1024, pixel size=0.24 dec93: CCD Thompson 1024x1024, pixel size=0.48 (0.24 2x2 binned) feb94: CCD Thompson 1024x1024, pixel size=0.24 (the observations in the x filter were done with an unknown filter, because of a mechanical fault). dec94: CCD Tektronics 1024x1024, pixel size=0.30 feb95: CCD Tektronics 1024x1024, pixel size=0.30 --- Filt Filter --- Exp Exposure time min FWHM Seeing arcsec Notes Notes --- Galaxies classified as S from visual inspection of the plates OCA2842 and OCA2849 (all but two not presented in Paper I) GMP GMP (Cat. <VIII.42>) galaxy number --- GMPa Abriged (Cat. <VIII.42>) galaxy number --- Char Characteristics --- Obs Other observations number=1 BO= Butcher & Oemler (1985ApJS...57..665B) GavI= Gavazzi, Garilli & Boselli (1990A&AS...83..399G ) GavIII= Gavazzi & Randone (1994), Cat. <J/A+AS/107/285> GavIV= Gavazzi, Boselli & Carrasco (1995), Cat. <J/A+AS/112/257> D80= Dressler (1980), Cat. <VII/174> kp1608= KPNO photographic plate (see Paper I) run 7= CCD observations in March 1993 (see Paper I) --- Note Notes number=1 BO= Butcher & Oemler (1985ApJS...57..665B) GavI= Gavazzi, Garilli & Boselli (1990A&AS...83..399G ) GavIII= Gavazzi & Randone (1994), Cat. <J/A+AS/107/285> GavIV= Gavazzi, Boselli & Carrasco (1995), Cat. <J/A+AS/112/257> D80= Dressler (1980), Cat. <VII/174> kp1608= KPNO photographic plate (see Paper I) run 7= CCD observations in March 1993 (see Paper I) --- Morphological description of spiral galaxies in Perseus Name Name --- Palomar Appearance on the Digitized Palomar Sky Survey --- OCA2977 Appearance on plate OCA #2977 --- n_OCA2977 Note on OCA2977 --- CCD Appearance on CCD image --- Run Run number --- Notes Notes number=1 For Zw 541-3, embedded in the halo of a bright star, out of redshift limits --- Morphological description of early-type galaxies in Coma GMPa Number in the abridged version of GMP catalogue <VII/42> --- GMP Number in the unabridged version of GMP catalogue <VII/42> --- Dress Number in Dressler's catalogue (Dressler 1980, <VII/174>). --- Name Usual designation, such as NGC, IC (Dreyer 1888, <VII/118>), and RB (Rood & Baum, 1967AJ.....72..398R) numbers. --- Vmag Asymptotic magnitude, in V (Johnson) mag log(Reff) Logarithm of the effective radius arcsec log(a) Logarithm of the semi major axis of the effective isophote arcsec SuBr Mean surface brightness inside the effective isophote, in V magnitude mag/arcmin2 Diskp Photometric evidence for a disk number=1 st: strong cl: clear ft: faint no: none. --- b/a Typical axis ratio number=2 Typical value, either its minimum value, if clearly defined, or its value at the effective isophote otherwise. --- n_b/a Location where axis ratio was estimated number=3 ex: at its extremum re: at the effective isophote co: if the value is the same at both locations. --- e4 Typical e_4_ parameter number=4 Typical value, either its extremum value, if clearly defined, or its value at the effective isophote otherwise. The estimates are in %. % n_e4 Location where e_4_ was estimated number=3 ex: at its extremum re: at the effective isophote co: if the value is the same at both locations. --- b/ae Axis ratio in the envelope, i.e. at the isophote {mu}_V_=24.85mag/arcsec^2^. --- Ampli Amplitude of isophotal twist in the range of reliable measurements deg Bar Detection of a bar number=5 bar: bar seen bar?: bar suspected -no: no bar seen. --- Disk Detection and classification of a disk number=6 emDi: embedded disk miDi: mixed disk exDi: extended disk -?Di: detected but unclassified disk -no-: no disk seen. --- Spiral Detection of a spiral pattern number=7 spiP: spiral pattern seen spiP?: spiral pattern suspected -no-: no spiral pattern seen. --- Envelope Classification of an envelope number=8 spH: spheroidal halo thD: thick disk exD: extended disk pec: peculiar envelope -?-: unclassified envelope. --- MType Our morphological classification number=9 boE: boxy E unE: undetermined E diE: disky E SA0, SAB0, SB0, Sa, etc., S...: spiral of unknown stage. --- Note An asterisk refers to a note number=10 Individual notes 0552: dust along the major axis. Type given in Paper I confirmed. 0718: two bumps on the major axis profile. Inner ring and lens. Type given in Paper I confirmed. 0750R: image of run 9 (see Paper I). 0750: 30 degree twist at r ~10 arcsec on the V image. same twist in R, but image not deep enough for full confirmation. Type given in Paper I confirmed. 0754: type given in Paper I fully confirmed. 0828: E boxy outside r_e_ and possibly disky inside. In Paper I it is classified diE because the boxiness of the outer region is not detected with certainty, partly because of the presence of a companion galaxy at 15 arcsec in the minor axis direction. 0857: the bar suspected in Paper I is not detected in our better images. 0908: slightly boxy isophotes out to r_e_, then slightly disky isophotes. Uncertain detailed classification. 0967: focus problems made the PSF slightly elongated in the NS direction and galaxy data inside 3 arcsec not usable. 1109: the bar suspected in Paper I is detected. 1154: asymmetric with respect to its major axis. 1432: classified SA0/a by morphologists, probably because of the low contrast spiP. 1564: ellipticity and e_4_ profile unusual for a lenticular galaxy. It seems to be asymmetric. 1594: the better data with respect to Paper I allow us to classify it elliptical. 1625: the bar suspected in Paper I is detected. 1844: isophote twist toward GMP 1852. Type given in Paper I confirmed. 1852: isophote twist opposite to GMP 1844, bar suspected but nearby star slightly elongated in the same direction. Type given in Paper I confirmed. 1925: large isophote twist at low SuBr. 2085: rich in globular clusters. The expression "globular cluster" here and hereafter does not imply a group of dynamically bound stars, but a clump of light.. The better data with respect to Paper I allow us to classify it elliptical. 2109: focus problems made the PSF slightly elongated in a direction orthogonal to the galaxy major axis. Data inside 4 arcsec are not usable. Also classified unE with CFH data of Paper I. 2134: rich in globular clusters. Its intensity profile obeys the r^-1.44^ law from 1 arcsec out to 60 arcsec, putting this galaxy in the D class following Schombert (1987IAUS..127..383S) and Tonry (1987IAUS..127...89T). Classified as unE in Paper I from a slightly shallower image. 2283: the analysis is made difficult by the crowded field and a nearby saturated star. --- Morphological description of early-type galaxies in Perseus Zw Zwicky name (Cat. <VII/49>) --- Name Usual designation, such as NGC, UGC (Nilson 1976, <VII/26>), T (Tifft 1978ApJ...222...54T), BGP (Bucknell et al. 1979MNRAS.188..579B), CR (Chincarini & Rood 1971ApJ...168..321C) --- ObsMat Flag for filter or observational material. --- mag Asymptotic magnitude. mag n_mag Note on mag number=1 A n means that the parameter has not been computed because the night was not photometric, or because of the pan-chromaticity of the plate. : is an uncertainty flag --- log(Reff) Logarithm of the effective radius arcsec log(a) Logarithm of the semi major axis of the effective isophote arcsec SuBr Mean surface brightness inside the effective isophote mag/arcmin2 n_SuBr Note on SuBr number=1 A n means that the parameter has not been computed because the night was not photometric, or because of the pan-chromaticity of the plate. : is an uncertainty flag --- Diskp Photometric evidence for a disk number=2 st: strong cl: clear ft: faint no: none. --- b/a Typical axis ratio number=3 Typical value, either its minimum value, if clearly defined, or its value at the effective isophote otherwise. --- n_b/a Location where axis ratio was estimated number=4 ex: at its extremum re: at the effective isophote co: if the value is the same at both locations. --- e4 Typical e_4_ parameter number=5 Typical value, either its extremum value, if clearly defined, or its value at the effective isophote otherwise. The estimates are in %. % n_e4 Location where e_4_ was estimated number=4 ex: at its extremum re: at the effective isophote co: if the value is the same at both locations. --- b/ae Axis ratio in the envelope, i.e. at the isophote V_=24.85 or R=24mag/arcsec^2^. --- n_b/ae Note on b/ae number=1 A n means that the parameter has not been computed because the night was not photometric, or because of the pan-chromaticity of the plate. : is an uncertainty flag --- Ampli Amplitude of isophotal twist in the range of reliable measurements deg u_Ampli Uncertainty flag on Ampli --- Bar Detection of a bar number=6 bar: bar seen bar?: bar suspected -no: no bar seen. --- Disk Detection and classification of a disk number=7 emDi: embedded disk miDi: mixed disk exDi: extended disk -?Di: detected but unclassified disk -no-: no disk seen. --- Spiral Detection of a spiral pattern number=8 spiP: spiral pattern seen spiP?: spiral pattern suspected -no-: no spiral pattern seen. --- Envelope Classification of an envelope number=9 spH: spheroidal halo thD: thick disk exD: extended disk pec: peculiar envelope -?-: unclassified envelope. --- MType Our morphological classification number=10 boE: boxy E unE: undetermined E diE: disky E SA0, SAB0, SB0, Sa, etc., S...: spiral of unknown stage. --- Note An asterisk refers to a note number=11 Individual notes T40: the identification of Tiff 40 is doubtful. The observed galaxy is the nearest one to the Tiff 40 coordinates. A brighter (spiral) galaxy is 4 arcmin SE, which is more likely Tiff 40, if we believe Kent & Sargent's (1983AJ.....88..697K) classification (S). 540-32: companion of NGC 1177, roundish. 540-33: peanut shaped SA0. 540-41: face on. 540-46: the small field of view did not allow us to image the whole envelope 540-57: there is a bump on the major axis SuBr profile at V=23 mag arcsec^2^ 540-73: this galaxy is 19 arcsec from a very bright star, preventing the detailed structural analysis. However, bulge and disk are clearly visually detected as a change of axis ratio and as a bump on the major axis profile, leading to our estimated type. The galaxy is edge-on. 540-74: our morphological type fully confirms that of Poulain, Nieto & Davoust (1992A&AS...95..129P). 540-76: strong, but smooth, dust lane on major axis. A second faint dust lane is present with an inclination of about 10 degrees with respect to the galaxy major axis 10 arcsec Southward. 540-81: dust just in the inner part of this galaxy observed near the CCD's edge. 540-89: a very bright star 20 arcsec from the galaxy center perturbs the isophotal analysis at that radius. e_4_ never dominates the Fourier terms, f_4_ asymmetry. 540-106: almost edge-on, a bit S-shaped, asymmetric. 540-114: the c/a profile starts to rise at fainter SuBr than sampled by plate, thus explaining the difference in the envelope classification. 541-15S: face on. 541-16N: the galaxy Zw 540-16S and nearby stars prevented us from measuring the shape of this galaxy's envelope. 541-16S: the galaxy 540-16N makes it impossible to measure the SuBr profile at r>12 arcsec. --- tables.tex LaTeX version of the tables comafig.ps Galaxies in the Coma sample persfig.ps Galaxies of the Perseus sample Patricia Bauer CDS 1997 Feb 19 Stefano Andreon <andreon@cerere.na.astro.it> J_A+AS_126_67.xml CCD photometry of late-type stars in the young open cluster IC 2602 J/A+AS/126/81 J/A+AS/126/81 IC 2602 VRI photometry CCD photometry of late-type stars in the young open cluster IC 2602 D C Foster P B Byrne S L Hawley W R J Rolleston Astron. Astrophys. Suppl. Ser. 126 81 1997 1997A&AS..126...81F Clusters, open Photometry, CCD Photometry, VRI open clusters and associations: individual (IC 2602) stars: evolution stars: late-type We present the results of VRI photometry of the young open cluster IC 2602. Two 15x15arcmin^2^ fields were observed in February and May 1991 using the 1-m Swope telescope at Las Campanas. Using theoretical isochrones obtained from D'Antona & Mazzitelli (1994ApJS...90..467D), and allowing for observational and other uncertainties, we identify 78 primary candidate members with 12<V<18.5 from their positions on colour-magnitude diagrams. We compare the cluster field with an offset field of similar galactic latitude and estimate the contamination due to background stars to be large, >=50%, as might be expected given its low galactic latitude. We also compare our photometry with that given for the X-ray detected stars of Randich et al. (1995A&A...300..134R) present complimentary narrow band H{alpha} photometry for a subset of the stars.
IC 2602 10 43.2 -64 24
A list of primary candidate members of IC2602 ID Star identification --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Vmag V magnitude mag V-R V-R color index mag V-I color index mag table3.tex LaTeX version of table3 Patricia Bauer CDS 1997 Mar 04 Duncan Foster <dcf@star.arm.ac.uk> J_A+AS_126_81.xml Penetrating the "zone of avoidance" V. An optical survey for hidden galaxies in the region 90<=l<=110, -10<=b<=+10 J/A+AS/127/101 J/A+AS/127/101 Galaxies in the "zone of avoidance". V. Penetrating the "zone of avoidance" V. An optical survey for hidden galaxies in the region 90<=l<=110, -10<=b<=+10 R Seeberger W Saurer Astron. Astrophys. Suppl. Ser. 127 101 1998 1998A&AS..127..101S J/A+AS/110/269 : Paper I., |b| = 5 (Weinberger+ 1995) J/A+AS/117/1 : Paper II., 180<l<240 (Seeberger+ 1996) J/A+AS/117/369 : Paper III. 120<l<130, |b|<10 (Lercher+ 1996) J/A+AS/126/247 : Paper IV., 130<l<180, |b|<5 (Saurer+ 1997) Cross identifications Galaxy catalogs catalogs dust, extinction galaxies: general large-scale structure of universe As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}<=l<=110{deg}, -10{deg}<=b<=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).
Optically detected galaxies in the region 90{deg}<l<110{deg}, |b|<10{deg} Name Object designation based on galactic position --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin RA2000h Right ascension (2000) h RA2000m Right ascension (2000) min RA2000s Right ascension (2000) s DE2000d Declination (2000) deg DE2000m Declination (2000) arcmin POSS POSS print number --- xpos Cartesian x-coordinate on POSS mm ypos Cartesian y-coordinate on POSS mm DmajE Maximum diameter on POSS-E arcmin DmajEc Maximum diameter of the core on POSS-E arcmin DmajO Maximum diameter on POSS-O arcmin DmajOc Maximum diameter of the core on POSS-O arcmin Ident Cross-identifications and remarks --- Patricia Bauer CDS 1997 Sep 25 Walter Saurer <walter@ast6.uibk.ac.at> J_A+AS_127_101.xml A catalogue of spatially resolved kinematics of galaxies: Bibliography J/A+AS/127/117 J/A+AS/127/117 Kinematics of galaxies A catalogue of spatially resolved kinematics of galaxies: Bibliography P Prugniel A Zasov G Busarello F Simien Astron. Astrophys. Suppl. Ser. 127 117 1998 1998A&AS..127..117P J/A+AS/122/521 : Kinematical data on early-type galaxies. I. (Simien+ 1997) J/A+AS/126/15 : Kinematical data on early-type galaxies. II. (Simien+ 1997) Bibliography Galaxy catalogs catalogs galaxies: general galaxies: kinematics and dynamics We present a catalogue of galaxies for which spatially resolved data on their internal kinematics have been published; there is no a priori restriction regarding their morphological type. The catalogue lists the references to the articles where the data are published, as well as a coded description of these data: observed emission or absorption line, velocity or velocity dispersion, radial profile or 2D field, observed position angle. This catalogue will be updated. Check for recent version at the URL: http://www-obs.univ-lyon1.fr/~prugniel/cgi-bin/hypercat/
Catalogue Name Normalized galaxy identifier The Name has been adopted by descending the hierarchy: (1) Usual name for the dSph and the Milky Way (2) NGC (Cat. <VII/118>) name (3) IC (Cat. <VII/118>) (4) UGC (Cat. <VII/26>) or ESO (Cat. <VII/34>) (5) PGC (Principal Galaxies Catalogue, Cat. <VII/119>) (Lyon-Meudon Extragalactic Database) internal identifier, also acronymed PGC (with numbers greater then 73097). The objects left unfolded into this hierarchy are designated as in the original publication. --- Oname Name in original publication --- RAh Right ascension (1950) hours h RAm Right ascension (1950) minutes min RAs Right ascension (1950) seconds s DE- Sign of declination --- DEd Declination (1950) degrees deg DEm Declination (1950) minutes arcmin DEs Declination (1950) seconds arcsec Bibcode CDS/ADS reference code --- Dom O: Optical; R: Radio --- Comp A: Absorption; E: Emission --- Dim Dimension --- Data V: Velocity; D: Dispersion; P: Position-velocity diagram; C: Channel map --- Axis MJ: Major; MI: Minor; PA: Connecting line BA: Along bar --- PA Position Angle the value "999" stands for "not available", and blanks mean "Meaningless" deg LineCode Codes of the observed lines, see table3 --- Bibliograplic references for table1 Bibcode CDS/ADS reference code --- Refer Bibliographic reference --- Spectral lines coding LineCode Code --- LineName Name of the line --- Wavel Wavelength with unit --- Patricia Bauer CDS 1997 Oct 14 Philippe Prugniel <prugniel@cumulus.univ-lyon1.fr> J_A+AS_127_117.xml A radio continuum study of the Magellanic Clouds. VI. Discrete sources common to radio and X-ray surveys of the Magellanic Clouds. J/A+AS/127/119 J/A+AS/127/119 Radio continuum study of the MC A radio continuum study of the Magellanic Clouds. VI. Discrete sources common to radio and X-ray surveys of the Magellanic Clouds. M D Filipovic W Pietsch R F Haynes G L White P A Jones R Wielebinski U Klein K Dennerl P T Kahabka J S Lazendic Astron. Astrophys. Suppl. Ser. 127 119 1998 1998A&AS..127..119F IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) IX/11 : ROSAT PSPC Source Catalog (Voges+ 1994) J/A+AS/111/311 : Radio continuum study of the MC (Filipovic+, 1995) J/A+AS/120/77 : Radio continuum study of the MC (Filipovic+, 1996) J/A+AS/121/321 : SMC catalogue of radiosources (Filipovic+ 1997) Haynes et al., Paper I. 1991A&A...252..475H Xu et al., Paper II. 1992A&A...257...47X Kelin et al., Paper III. 1993A&A...271..402K Filipovic et al., Paper IV. 1995A&AS..111..311F, Cat. <J/A+AS/111/311> Filipovic et al., Paper IVa. 1996A&AS..120...77F, Cat. <J/A+AS/120/77> Filipovic et al., Paper V. 1997A&AS..121..321F, Cat. <J/A+AS/121/321> Filipovic et al., Paper VI. 1998A&AS..127..119F Magellanic Clouds Radio sources X-ray sources HII regions Magellanic Clouds radio continuum: galaxies supernova remnants X-rays: galaxies By comparing Parkes telescope radio surveys with the X-ray ROSAT All-Sky Survey (RASS) we have found 71 discrete sources of both radio and X-ray emission in the Large Magellanic Cloud (LMC). These 71 sources are mainly supernova remnants (SNRs) and SNR candidates (36), and background sources (27). For six of the sources we have no proposed identification and the other two are HII regions. A source-intensity comparison of the radio and X-ray sources shows very little correlation, but we note that the strongest SNRs at both radio and X-ray frequencies are young SNRs from Population I. Six new LMC SNR candidates are proposed. From the radio flux density of the SNRs we have estimated the SNR birth rate to be one every 100 (+/-20) yr and the star-formation rate (SFR) to be 0.7 (+/-0.2)M_{sun}_/yr. A similar comparison was undertaken for the Small Magellanic Cloud (SMC), but instead of the RASS we used a roster of pointed observations made with the ROSAT Position Sensitive Proportional Counter (PSPC). This comparison resulted in 27 sources in common between the Parkes radio and ROSAT PSPC surveys. Two new SMC sources are proposed for SNR candidates. The SMC SNR birth rate was estimated to be one every 350 (+/-70)yr and the SFR was estimated to be 0.15 (+/-0.05)M_{sun}_/yr.
Catalogue of the LMC radio sources identified in the RASS Catalogue of the SMC radio sources identified in the ROSAT PSPC (Cat. <IX/11>) Seq Sequential number --- RadioName Radio source name --- X-rayName X-ray source name number=1 The X-ray source name is taken from Pietsch et al. (in prep.) in table2.dat and from Kahabka et al. (in prep.) in table3.dat. More details are given in Sect. 3. --- S4.75GHz Radio flux density at 4.75 GHz for LMC and 4.85GHz for SMC Jy n_S4.75GHz f: flux density estimated by interpolation from other radio frequencies --- CR Count Rate ct.k/s alpha Source radio spectral index number=2 In order to extend the radio frequency coverage and to obtain more accurate radio spectral indices we have also used some flux densities from other radio catalogues; Clarke et al. (1976AuJPS..40....1C) at 0.408GHz, Mills et al. (1984AuJPh..37..321M) at 0.843GHz and Milne et al. (1980MNRAS.191..469M) at 14.7GHz. Spectral indices are not given for 10 LMC and six SMC sources which were detected at only one radio frequency or for which radio data are only available at two close frequencies (4.75GHz and 4.85GHz). --- e_alpha Error in alpha --- HR2 Hardness ratio HR2 --- Type Radio type source number=3 BG, bg: background sources Hii : H II regions SNR, snr : Supernova remnant SNR1: evolved SNRs SNR2: Oxygen-rich SNRs SNR3: Balmer-dominated SNRs SNR4: Crab-like SNRs SNR5: possible type III SNRs Capitals (BG, SNR and Hii) were used for classifications from previous works and lower case (bg and snr) for sources classified here The question-mark indicates probable but not certain classification. --- r_Seq References detailed in file refs.dat --- References for table2.dat and table3.dat Ref Reference number --- Text Text of Reference --- LMC cross-identifications SMC cross-identifications Seq Sequential number --- Names Other names --- Com Comments number=1 Abbreviations used: N H{alpha} catalogue of emission nebulae (Henize, 1955ApJS....2..315H) MC Radio catalogue (5.00 GHz) (McGee et al., 1972AuJPh..25..581M) MC4 Radio catalogue (0.408 GHz) (Clarke et al., 1976MNRAS.174..393C) DEM L H{alpha} catalogue of emission nebulae (Davies et al., 1976MmRAS..81...89D) DEM S H{alpha} catalogue of emission nebulae (Davies et al., 1976MmRAS..81...89D) NGC NGC 2000 catalogue (optical) (Sinnott, 1988, Cat. <VII/118>) LHG Einstein X-ray catalogue (Long et al., 1981ApJ...248..925L) W Einstein X-ray catalogue (Wang et al., 1991ApJ...374..475W) PSR Catalogue of pulsars (Taylor et al., 1993, Cat. <VII/156>) PMN Radio catalogue (4.85 GHz) (Wright et al., 1994, Cat. <VIII/38>) PKS PKSCAT-90 radio catalogue (Otrupcek & Wright, 1991PASAu...9..170O) Sa Catalogue of planetary nebula (Sanduleak et al., 1978PASP...90..621S; Sanduleak, 1984IAUS..108..231S) CO Catalogue of CO molecular clouds (Cohen et al., 1988ApJ...331L..95C) IJL Catalogue of CO molecular clouds (Israel et al., 1993, Cat. <J/A/A/276/25>) LH Catalogue of stellar associations (Lucke & Hodge, 1970AJ.....75..171L) S Radio catalogue (McGee et al., 1976AuJPh..29..329M) MRC Radio catalogue (408 MHz) (Large et al., 1981, Cat. <VIII/16>) E X-ray catalogue (Seward & Mitchell, 1981ApJ...243..736S) IKT X-ray catalogue (Inoue et al., 1983IAUS..101..535I) LI-SMC IR catalogue (Schwering & Israel, 1991A&A...246..231S; Israel et al., 1993, Cat. <J/A/A/276/25>) WW X-ray catalogue (Wang & Wu, 1992ApJS...78..391W) BKGS X-ray catalogue (Bruhweiler et al., 1987ApJ...317..152B) --- tables.tex LaTeX version of the tables tables.ps Post-Script version of the tables Patricia Bauer CDS 1998 Feb 19 Miroslav Filipovic <fica@mpe.mpg.de> J_A+AS_127_119.xml V,I CCD photometry of metal-rich globular clusters: NGC 6528 J/A+AS/127/167 J/A+AS/127/167 V,I CCD photometry of NGC 6528 V,I CCD photometry of metal-rich globular clusters: NGC 6528 T Richtler E K Grebel A Subramaniam R Sagar Astron. Astrophys. Suppl. Ser. 127 167 1998 1998A&AS..127..167R Clusters, globular Photometry, CCD Galaxy: abundances globular clusters: general globular clusters: individual (NGC 6528) Hertzsprung-Russell (HR diagram) We present CCD photometry in V and I for the metal-rich globular cluster NGC 6528. A comparison with previous photometry reveals discrepancies of the order 0.1 to 0.2mag in V, emphasizing the need for independent photometry. As found previously, the giant branch (or the asymptotic giant branch, which cannot be distinguished) of the cluster extends to V-I=7. Population synthesis in V-I must take these red stars into account in order to understand integrated red colours of bulge populations. Currently available theoretical isochrones do not reproduce the shape of the RGB/AGB. The derivation of reliable values for reddening, distance and metallicity of NGC 6528 is hampered by uncertainties in the extrapolation to high metallicity, which dominate the absolute error rather than the photo metric uncertainty does. Together with other properties (old age derived from HST data, high radial velocity), this object is more likely a member of the bulge than of the disk population.
NGC 6528 18 04 49.5 -30 03 21
Position and photometry of 24999 stars in a field of view of 5.7'x5.7' Seq Sequential number --- Xpos X position number=1 the pixel size is 0.332arcsec, North up, West right. pix ypos Y position number=1 the pixel size is 0.332arcsec, North up, West right. pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag V-I V-I colour index mag e_V-I rms uncertainty on V-I mag Chi chi-value returned from DAOPHOT --- Patricia Bauer CDS 1997 Jun 12 Tom Richtler <richtler@astro.uni-bonn.de> J_A+AS_127_167.xml New detections of H2O maser sources on the 13.7m radio telescope of Purple Mountain Observatory J/A+AS/127/181 J/A+AS/127/181 H2O maser sources new detections New detections of H2O maser sources on the 13.7m radio telescope of Purple Mountain Observatory F Han R Q Mao J Lu Y F Wu J Sun J S Wang C C Pei Y Fan G S Tang H R Ji Astron. Astrophys. Suppl. Ser. 127 181 1998 1998A&AS..127..181H Masers Radio lines masers radio lines: ISM Observations of H_2_O maser sources on the 13.7m radio telescope of Purple Mountain Observatory from 1990 Aug. to 1994 Jan. are summarized. For searching new water masers, the total number of search candidates is about 360, with 110 objects detected. Among them are 96 new detections. A list of the new detections and their spectra are presented.
Parameters of the new water maser sources Source Source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Class Class of the source --- Flux Flux density of the strongest component Jy Vlsr Peak velocity with respect to LSR km/s rms Noise level of the spectrum Jy S Integrated flux Jy.km/s Date Date of observation "DD/MM/YY" table1.tex LaTeX version of table1 fig1-1.ps Maser spectra fig1-2.ps Fig. 1 continued fig1-3.ps Fig. 1 continued fig1-4.ps Fig. 1 continued fig1-5.ps Fig. 1 continued fig1-6.ps Fig. 1 continued fig1-7.ps Fig. 1 continued fig1-8.ps Fig. 1 continued fig1-9.ps Fig. 1 continued fig1-10.ps Fig. 1 continued R.Q. Mao Purple Mountain Observatory Patricia Bauer CDS 1997 May 15 Mao Ruiqing, <pmoyl@pub.nj-online.nj.js.cn> J_A+AS_127_181.xml SiO masers in OH/IR stars, proto-planetary and planetary nebulae J/A+AS/127/185 J/A+AS/127/185 SiO masers in OH/IR stars, proto-PN and PN SiO masers in OH/IR stars, proto-planetary and planetary nebulae L -A Nyman P J Hall H Olofsson Astron. Astrophys. Suppl. Ser. 127 185 1998 1998A&AS..127..185N Masers Planetary nebulae masers radio lines: stars stars: AGB and post-AGB We present a search for SiO masers towards a sample of 126 objects including OH/IR stars, proto-planetary and planetary nebulae. All objects are classified as oxygen-rich, and most of them are associated with OH or H_2_O masers. SiO masers were found only in variable objects like the OH/IR stars and a few objects classified as proto-planetary nebulae, but with variable central stars that may be part of binary systems. In one object, OH 15.7+0.8, which appears to be varying irregularly and most likely recently left the AGB, an SiO maser was tentatively detected. Thus, we conclude that variability and SiO maser emission are closely linked, and that SiO masers disappear very soon after a star has reached the end of the AGB, when pulsation and mass loss cease.
Source parameters IRAS IRAS name --- Names Other name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vlsr LSR center velocity of the spectra km/s OH x: Presence of OH --- H2O x: Presence of H2O --- SiO x: Presence of SiO, X: new detection --- Type Evolutionary status of the object number=1 OH/IR: objects with double-peaked OH spectra that have been found to have variable OH, and/or optical, and/or infrared emission. If no special monitor observations have been reported in the literature, we regard an object as variable if the IRAS variability index is>90. None of the characteristics given below for PPNe have been reported for these objects. PPN: objects that have one or more of the following characteristics: bipolar appearance, an early type central star, a double peaked energy distribution, high velocity masers, and/or the velocity width of the H_2_O emission exceeds that of the OH emission. PN: Objects that have been detected in radio continuum, indicating the presence of ionized gas. variable star: Two objects where OH maser emission has not been detected, but with variable central stars supergiant: Two objects: IRAS 22480+6002 that has been classified as a supergiant and IRC+10420 which may be a post-AGB object or a supergiant. PMS?: Five of the objects are more likely to be pre-main sequence objects than evolved objects. These definitions cover 86% of the sample. ?: The rest of the objects that do not fit into the above criteria because of lack of relevant observations. We have not made any attempt to separate them into possible OH/IR objects or PPNe, although most of them probably are OH/IR objects. --- r_Type References detailed in table refs.dat --- SiO maser observations IRAS IRAS name --- HJD1 Epoch of observation of SiO v=1, J=1-0 d rms1 rms of SiO v=1, J=1-0 Jy peak1 Peak flux for SiO v=1, J=1-0 number=1 Only the peak flux is given for tentatively detected sources. Jy Int1 Int of SiO v=1, J=1-0 10-20W/m2 HJD2 Epoch of observation of SiO v=2, J=1-0 d u_rms2 *: Calibration is uncertain due to unstable weather --- rms2 rms of SiO v=2, J=1-0 Jy peak2 Peak flux for SiO v=2, J=1-0 number=1 Only the peak flux is given for tentatively detected sources. Jy Int2 Int of SiO v=2, J=1-0 10-20W/m2 n_HJD3 *: Observation of SiO (2-1) made with the Onsala 20 m telescope --- HJD3 Epoch of observation of SiO v=1, J=2-1 d rms3 rms of SiO v=1, J=2-1 Jy peak3 Peak flux for SiO v=1, J=2-1 number=1 Only the peak flux is given for tentatively detected sources. Jy Int3 Int of SiO v=1, J=2-1 10-20W/m2 References RefNo Reference number --- Text Text of reference, including the Bibcode --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Jul 18 Lars-Ake Nyman <lnyman@puppis.ls.eso.org> J_A+AS_127_185.xml The 1997 reference of diffuse night sky brightness J/A+AS/127/1 J/A+AS/127/1 1997 reference of diffuse night sky brightness The 1997 reference of diffuse night sky brightness C Leinert S Bowyer L K Haikala M S Hanner M G Hauser A -C Levasseur-Regourd I Mann K Mattila W T Reach W Schlosser H J Staude G N Toller J L Weiland J L Weinberg A N Witt Astron. Astrophys. Suppl. Ser. 127 1 1998 1998A&AS..127....1L J/A+AS/112/99 : Calar Alto Obs. sky brightness (Leinert+, 1995) J/A+AS/119/153 : La Silla Observatory sky brightness 1978-1988 (Mattila+ 1996) Earth References astronomical data bases: miscellaneous atmospheric effects diffuse radiation infrared: general interplanetary medium ultraviolet: general In the following we present material in tabular and graphical form, with the aim to allow the non-specialist to obtain a realistic estimate of the diffuse night sky brightness over a wide range of wavelengths from the far UV longward of Ly{alpha} to the far-infrared. At the same time the data are to provide a reference for cases in which background brightness has to be discussed, including the planning for space observations and the issue of protection of observatory sites. We try to give a critical presentation of the status at the beginning of 1997.
References Ref Reference code --- --- --- BibCode Bibcode --- Aut Autors names and comments --- map0060.fit *Galactic diffuse emission at a wavelength of 60{mu}m in ecliptic coordinates (table41 in section 11.4 of the paper) map0100.fit *Galactic diffuse emission at a wavelength of 100{mu}m in ecliptic coordinates (table42 in section 11.4 of the paper) Patricia Bauer CDS 1997 Dec 12 Christoph Leinert <leinert@mpia-hd.mpg.de> J_A+AS_127_1.xml Variations of Ap stars in the Geneva system J/A+AS/127/201 J/A+AS/127/201 Variations of Ap stars in the Geneva system Variations of Ap stars in the Geneva system J Manfroid M Burnet P Renson Astron. Astrophys. Suppl. Ser. 127 201 1998 1998A&AS..127..201M Photometry, Geneva Stars, Ap stars: chemically peculiar stars: variables: general The photometric behaviour of 21 Ap stars has been analyzed from observations obtained in the Geneva system. Variability has been detected for 9 Ap stars, as well as for a star which initially was a comparison star. Preliminary values for the periods are presented as well as an analytical description of the light curves. The material has been collected during a 23-night observing run at La Silla with the 70cm telescope of the Geneva Observatory equipped with the standard Geneva photometer. The parameters of a second-order cosine fit to the lightcurves are stored in the accompanying table. Time origin is JD 2450000.0. The 17 phase diagrams for each of the 9 stars are presented in 9 postscript files. The observational data are superimposed on the Fourier fit. Data are differential, except for HD 191439 and HD 192674 which had no suitable comparisons.
HD 8717 01 25 27.4 -28 46 56 HD 9906 01 36 08.0 -29 54 29 HD 162515 17 52 55.7 -35 01 07 HD 187923 19 52 04.5 +11 37 59 HD 188309 19 54 02.8 +13 16 18 HD 191439 20 12 57.5 -58 46 44 HD 192674 20 18 19.3 -51 05 12 HD 192687 20 15 42.3 +13 50 57 HD 194750 20 29 02.2 -43 14 57 HD 195112 20 30 45.4 -38 34 40 HD 199288 20 57 42.3 -44 06 56 HD 200623 21 05 34.7 -35 42 08 HD 201901 21 13 16.9 -27 37 04 HD 203608 21 26 25.9 -65 22 39 HD 207259 21 51 43.2 -73 10 08
Variations of Ap stars in the Geneva system HD HD (Cat. <III/135>) number --- Per Period d Index Index/magnitude number=1 Code to the Geneva magnitudes or indices 1: V 2: U-B 3: V-B 4: B1-B 5: B2-B 6: V1-B 7: G-B 8: U 9: B 10: B1 11: B2 12: V1 13: G 14: B1-B2 15: B2-V1 16: V1-G 17: B1-V1 --- B1 Amplitude of fundamental cosine component (see Eq. 1 in article) mag e_B1 Error on B1 mag B2 Amplitude of harmonic mag e_B2 Error on B2 mag PHI1 Phase of fundamental component computed with time origin = JD 2450000 rad e_PHI1 Error on PHI1 rad PHI2 Phase of harmonic rad e_PHI2 Error on PHI2 rad RMS Scatter around the analytical fit mag R Total range of analytical light curve mag S/N Signal-to-noise ratio --- 008717.ps Phase diagram for HD 8717, with comp. HD 9906 188309.ps Phase diagram for HD 188309, with comp. HD 162515 and 187923 191439.ps Phase diagram for HD 191439 192674.ps Phase diagram for HD 192674 192687.ps Phase diagram for HD 192687, with comp. HD 162515 and 187923 194750.ps Phase diagram for HD 194750, with comp. HD 199288 195112.ps Phase diagram for HD 195112, with comp. HD 199288 200623.ps Phase diagram for HD 200623, with comp. HD 201901 207259.ps Phase diagram for HD 207259, with comp. HD 203608 Patricia Bauer CDS 1997 Aug 25 Jean Manfroid <manfroid@astra.astro.ulg.ac.be> J_A+AS_127_201.xml The absorption spectrum of the QSO PKS 2126-158 (z_em_=3.27) at high resolution J/A+AS/127/217 J/A+AS/127/217 Absorption spectrum of the QSO PKS2126-158 The absorption spectrum of the QSO PKS 2126-158 (z_em_=3.27) at high resolution V D'Odorico S Cristiani S D'Odorico A Fontana E Giallongo Astron. Astrophys. Suppl. Ser. 127 217 1998 1998A&AS..127..217D QSOs Spectroscopy quasars: absorption lines quasars: individual (PSR 2126-158) Spectra of the z_em_=3.268 quasar PKS 2126-158 have been obtained in the wavelength range 430-662nm with a resolution R=27000 and an average signal to noise ratio s/n=25 per resolution element. 12 metal absorption systems have been identified, two of which were previously unknown. All the lines shortward of the Lyman{alpha} emission not identified as due to metals have been fitted as Lyman{alpha} and Lyman{beta}. We reported statistical analysis of this sample of lines. In particular, the two-point correlation function for metal systems has been computed.
PKS 2126-158 21 29 12.0 -15 38 42
Table of absorption lines No Number of the line --- lambda central wavelength 0.1nm b Doppler parameter km/s e_b rms uncertainty on Doppler parameter km/s logN Column density [cm-2] e_logN rms uncertainty on logN [cm-2] z Redshift -- ID Line identification -- table.tex LaTeX version of the table Valentina D'Odorico SISSA Patricia Bauer CDS 1997 Oct 16 Valentina D'Odorico <dodorico@sissa.it> J_A+AS_127_217.xml The ROSAT all-sky survey catalogue of optically bright late-type giants and supergiants J/A+AS/127/251 J/A+AS/127/251 Giants and supergiants ROSAT data The ROSAT all-sky survey catalogue of optically bright late-type giants and supergiants M Huensch J H M M Schmitt W Voges Astron. Astrophys. Suppl. Ser. 127 251 1998 1998A&AS..127..251H IX/11 : ROSAT PSPC Source Catalog (Voges+ 1994) Stars, giant Stars, supergiant X-ray sources catalogs stars: activity stars: coronae stars: late-type X-rays: stars We present X-ray data for all late-type (A,F,G,K,M) giants and supergiants (luminosity classes I to III-IV) listed in the Bright Star Catalogue that have been detected in the ROSAT all-sky survey. The selection of the sample stars, the data analysis, the criteria for an accepted match between star and X-ray source, and the determination of X-ray fluxes are described.
ROSAT
RASS detections of BSC late-type giants HRname Bright Star (Cat. <V/50>) number --- HD Henry Draper (Cat. <III/135>) number --- Name Star's name --- Vmag V magnitude mag B-V B-V colour index mag SpType MK spectral classification --- Binary Binary Flag number=1 S: Single VB: Visual binary SB: Spectroscopic binary RS: RS CVn system B: Other binary CV: Catalclysmic companion Symb: Symbiotic star --- ExpTime Effective exposure time s Count Mean PSPC count rate ct/s e_Count Error of PSPC count rate ct/s LEx Likelihood of existence --- Delta Offset between optical and X-ray position arcsec HR Hardness Ratio =(H-S)/(H+S) --- e_HR Error of Hardness Ratio --- FX Apparent X-ray flux (0.1-2.4 keV) 10-17W/m2 log(FX/Fbol) X-ray to bolometric flux ratio --- Patricia Bauer CDS 1997 May 22 Matthias Huensch <mhuensch@rosat.mpe-garching.mpg.de> J_A+AS_127_251.xml Are metallic A-F giants evolved Am stars? Rotation and rate of binaries among giant F stars J/A+AS/127/277 J/A+AS/127/277 Rotation and binary rate among giant F stars Are metallic A-F giants evolved Am stars? Rotation and rate of binaries among giant F stars M Kuenzli P North Astron. Astrophys. Suppl. Ser. 127 277 1998 1998A&AS..127..277K Binaries, spectroscopic Radial velocities Stars, F-type Stars, giant binaries: spectroscopic delta Scuti stars: chemically peculiar stars: evolution stars: rotation We have tested the hypothesis of Berthet (1991A&A...251..171B) which foresees that Am stars become giant metallic A and F stars (defined by an enhanced value of the blanketing parameter {delta}m2 of the Geneva photometry) when they evolved. If this hypothesis is right, Am and metallic A-FIII stars need to have the same rate of binaries and a similar distribution of vsini. From our new spectroscopic data and from vsini and radial velocities in the literature, we show that it is not the case. The metallic giant stars are often fast rotators with vsini larger than 100 km/s, while the maximum rotational velocity for Am stars is about 100 km/s. The rate of tight binaries with periods less than 1000 days is less than 30 % among metallic giants, which is incompatible with the value of 75 % for Am stars (Abt & Levy, 1985ApJS...59..229A). Therefore, the simplest way to explain the existence of giant metallic F stars is to suggest that all normal A and early F stars might go through a short "metallic" phase when they are finishing their life on the main sequence. Besides, it is shown that only giant stars with spectral type comprised between F0 and F6 may have a really enhanced {delta}m2 value, while all A-type giants seem to be normal.
Radial velocities of standard stars Radial velocities of A and F giants HD HD number number=1 Average values of radial velocity for table2 stars: ------------------------ Star <V_r_> ------------------------ HD 693 15.44+/-0.36 HD 22484 27.86+/-0.44 HD 89449 5.84+/-0.52 HD 114762 47.77+/-0.26 HD 136202 54.39+/-0.27 HD 187691 -0.27+/-0.49 HD 222368 5.12+/-0.45 ------------------------ --- HJD Heliocentric Julian day d RV Radial velocity km/s e_RV rms uncertainty on RV km/s Discussion about the duplicity of all photometric metallic F giant stars of Hauck (1986A&A...155..371H) Name HD number --- NTot Total number of lines for the reference --- Nline Running line number in range [1,Ntot] --- Com Comments number=1 References: Abt (1965ApJS...11..429A) Abt (1969ApJS...19..387A) Abt & Biggs, 1972, Bibliography of Stellar Radial Velocities, Latham Process Corp., New York Abt & Levy (1976ApJS...30..273A) Adams et al. (1929ApJ....70..207A) Breger (1979PASP...91....5B) Buscombe & Morris (1958MNRAS.118..609B) Campbell (1913LicOB...7..113C) Campbell (1928PLicO..16.....C) Cannon (1920PDO.....4..253C) Catchpole et al. (1982RGOB..188....5C) Evans (1961RGOB...44..351E) Evans (1966RGOB..110..185E) Evans et al. (1961RGOB...48..389E) Evans et al. (1964RGOB...85..207E) Evans et al. (1957MNRAS.117..534E) Frost et al. (1929PYerO...7....1F) Harper (1937PDAO....7....1H) Henroteau (1923PDO.....8...59H) Jones & Haslam (1969RGOB..155...19J) Mayor & Mazeh (1987A&A...171..157M) Nelson & Kreidl (1993AJ....105.1903N) Neubauer (1930LicOB..15...47N) Nordstroem & Andersen (1985A&AS...61...53N, Cat. <III/127>) Penfold (1971PASP...83..497P) Rodriguez et al. (1994A&AS..106...21R) Rosvick & Scarfe (1991PASP..103..628R) Sanford & Karr (1942ApJ....96..214S) Shajn & Albitzky (1932MNRAS..92..771S) Smith (1982ApJ...254..242S) Wilson & Joy (1950ApJ...111..221W) Wooley et al. (1971ROAn...14....1W) --- tables.tex LaTeX version of the tables Francois Ochsenbein CDS 1997 Jul 15 Marc Kunzli <marc.kunzli@obs.unige.ch> J_A+AS_127_277.xml The "Virgo photometry catalogue"; a catalogue of 1180 galaxies in the direction of the Virgo Cluster's core J/A+AS/127/367 J/A+AS/127/367 Virgo Photometry Catalogue The "Virgo photometry catalogue"; a catalogue of 1180 galaxies in the direction of the Virgo Cluster's core C K Young M J Currie Astron. Astrophys. Suppl. Ser. 127 367 1998 1998A&AS..127..367Y VII/48 : Catalogue of middle UV photometry of Virgo cluster galaxies J/A+AS/106/199 : B-band photometry in Fornax and Virgo (Caon+ 1994) J/A+AS/118/441 : Virgo + Fornax clusters galaxies UBVRI data (Schroeder+ 1996) J/A+AS/121/507 : Near-IR surface photometry of Virgo galaxies (Boselli+ 1997) Clusters, galaxy Galaxy catalogs Photometry, surface Radial velocities catalogs galaxies: clusters: individual (Virgo cluster) galaxies: fundamental parameters galaxies: photometry The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J_25=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue. Errata to printed version of paper: BAO has recently relocated, hence the new postcode. Beijing Astronomical Observatory Chinese Academy of Sciences Beijing 100012 China On p.377, for "r=10\frac{1}{10}r_0" read: "r=10_{\frac{1}{10}}r_0" On p.390, for "Young C.K., Galaxies. In: Chan K.C., Cheng K.S. (eds.)". read: "Young C.K., 1997, Galaxies. In Cheng K.S., Chan K.L. (eds.)". On p.390, for "Young C.K., Metcalfe N., Zhu J., Wu H., Chen J., A&A" read "Young C.K., Metcalfe N., Zhu J., Wu H., Chen J., A&AS, 130, 173".
*Main catalogue (AppenC) VPC Designation of galaxy in the VPC --- J9229i Photometry from Plate J9229 in VPC? number=1 1: yes; 0: no --- J4882i Photometry from Plate J4882 in VPC? number=1 1: yes; 0: no --- U9362i Photometry from Plate U9362 in VPC? number=1 1: yes; 0: no --- R2936i Photometry from Plate R2936 in VPC? number=1 1: yes; 0: no --- NGC/ICi Listed in NGC or IC (Cat. <VII/118>) ? number=2 'N': listed in NGC 'I': listed in IC ' ': not listed in either the NGC or IC --- NGC/IC NGC or IC designation number --- m_NGC/IC Multiplicity index on NGC/IC --- VCCi Listed in VCC (Binggeli et al., 1985AJ.....90.1681B)? number=4 'V': listed in VCC of Binggeli et al. (1985AJ.....90.1681B) ' ': not listed in VCC --- VCC VCC designation number --- n_VCC VCC membership assignment number=5 'm': member of the Virgo Cluster 'p': possible member of the cluster 'b': in the background --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min --- --- RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg --- --- DEm Declination (1950.0) arcmin --- --- DEs Declination (1950.0) arcsec RA2000h Right ascension (2000.0) h RA2000m Right ascension (2000.0) min --- --- RA2000s Right ascension (2000.0) s DE2000- Declination sign --- DE2000d Declination (2000.0) deg --- --- DE2000m Declination (2000.0) arcmin --- --- DE2000s Declination (2000.0) arcsec HRV Heliocentric radial velocity km/s e_HRV Standard error on velocity km/s r_HRV Source of velocity number=6 1: Karachentsev & Karachentseva (1982PAZh....8..198K) 2: Karachentsev et al. (1983PAZh....9..387K) 3: Binggeli et al. (1985AJ.....90.1681B) [VCC] 4: Rhee & Katgert (1988A&AS...72..243R) 5: de Vaucouleurs et al. (1991, Cat. <VII/155>) [RC3] 6: Binggeli et al. (1993A&AS...98..275B) 7: Drinkwater et al. (1996, Cat. <J/MNRAS/279/595>) New measurements already made as well as further ones will be added at a future date, hence two digits have been reserved for this field. --- MType Morphological type number=7 E': elliptical E?': elliptical? S': spiral S?': spiral? S0': lenticular S0?': lenticular? I': irregular I?': irregular? BCD': blue compact dwarf BCD?': blue compact dwarf? pre': pre-merger pec': peculiar ?': unknown or object defied classification Velocity data should be used in preference to types as indicators of cluster membership. Two VPC objects typed as 'BCD?' in the VCC (Binggeli et al., 1985AJ.....90.1681B) have since been found to be background objects--probably spirals. --- r_MType Source of type number=8 1: VCC (Binggeli et al., 1985AJ.....90.1681B) 2: VPC [this work] --- Btmag Total B magnitude mag r_Btmag Source of Bt number=9 1: Transformed value from VPC B_J_ and R_C_ photometry New measurements will be added at a future date for objects whose B_J_ and R_C_ VPC photometry was saturated. --- Eps Ellipticity (10) number=22 Ellipticities = 1-(B/A) where A & B are the major & minor diameters respectively. For any detailed study of Virgo galaxy orientations, it is recommended that the surface photometry itself is used rather than the values quoted in the main catalogue. This is because most of the ellipticities quoted in the main catalogue are arbitrarily based on the mu_B_J_24.25 isophote. Ellipticity does of course vary from isophote to isophote and from band to band. --- PAE Position angle for E measurement See notes (10) number=23 Position angles = that of the major axis measured from the meridian through East. deg BandE Pass-band for E measurement number=11 'u'; U band 'b': B band 'j': B_J_ band --- IsoE ubjr isophote for E measurement mag/arcsec2 U-Bj (U-B_J_) equal-area colour number=20 For an individual galaxy, equal-area colours are significantly more accurate than total colours derived from two total magnitude values. However, for the galaxy sample as a whole, the total colours are likely to suffer from less bias effects. mag e_U-Bj Standard error on U-B_J_ equal-area colour number=12 A standard error value is only quoted here if the relevant colour is based on the mean of two values [one from Plate U9362 or R2936 and J9229 and the other from U9362 or R2936 and J4882]. Each observed error was multiplied by the square root of 2 in order to obtain the quoted value. The quoted standard error therefore assumes [in the absence of additional U- or R_C_-band plates] that the errors in the U- or R_C_-band photometry are, for any particular galaxy, the same as those in B_J_. mag Bj-R (B_J_-R) equal-area colour mag e_Bj-R Standard error on B_J_-R equal-area colour number=12 A standard error value is only quoted here if the relevant colour is based on the mean of two values [one from Plate U9362 or R2936 and J9229 and the other from U9362 or R2936 and J4882]. Each observed error was multiplied by the square root of 2 in order to obtain the quoted value. The quoted standard error therefore assumes [in the absence of additional U- or R_C_-band plates] that the errors in the U- or R_C_-band photometry are, for any particular galaxy, the same as those in B_J_. mag Bj25 B_J_25 isophotal magnitude number=10 Mean value for both B_J_-band plates if applicable, otherwise just based on one plate. mag RadBj25 Mean radius of mu(B_J_)=25 isophote See notes (10) number=24 Mean radii= SQRT(A*B). arcsec SuBrBjc Measured central B_J_ surface brightness See note number=10 Mean value for both B_J_-band plates if applicable, otherwise just based on one plate. mag/arcsec2 SuBrBj25 Mean surface brightness for mu(B_J_)<=25 See note number=10 Mean value for both B_J_-band plates if applicable, otherwise just based on one plate. mag/arcsec2 Bjoverlap Brightest overlapping Bj isophote number=10 Mean value for both B_J_-band plates if applicable, otherwise just based on one plate. mag/arcsec2 BjTot B_J_t total magnitude (10) number=21 A total magnitude [and any total colour based on it] cannot be assumed to be reliable if the relevant n value= 0.20 or 3.00 or the relevant number of isophotal levels fitted = 4 or less, even if only one pass band is affected. mag BJRn Sersic parameter n_B_J_ (Plate J9229) --- Bj0 Extrapolated Sersic central B_J_ surface brightness (Plate J9229) mag/arcsec2 r0Bj Sersic scale length r_0_B_j_ (Plate J9229) arcsec NBj Number of B_J_ isophotes fitted --- r_Bj25 Source of non-VPC photometry Bj25 number=13 0: if derived from VPC photometry 1: de Vaucouleurs & Pence (1979ApJS...40..425D), table 2 2: de Vaucouleurs & Pence (1979ApJS...40..425D), table 4 3: Binggeli et al. (1984AJ.....89...64B) 4: VCC, Binggeli et al. (1985AJ.....90.1681B) 5: Karachentsev & Karachentseva (1982PAZh....8..198K) 6: average of sources 2 and 4 7: average of sources 4 and 5 9: this work, when estimate made by eye --- n_Bj25 Reliabilty of Bj25 number=14 ' ': if B_J_25 derived from VPC photometry (see paper for typical error values) 'R': if B_J_25 not from VPC photometry but reliable according to the VCC 'U': if B_J_25 not from VPC photometry and unreliable according to the VCC --- n_e_Bj25 [-] sign of the difference (15) or 9 when no value (99999) --- e_Bj25 Standard error on Bj25 number=15 A standard error value is only quoted if the relevant B_J_25 value is based on the mean of two values [one from each of the two B_J_-band plates]. The standard error is the modulus of the value quoted; the sign representing the sense of the difference: [ B_J_25(Plate J9229) minus B_J_25 (Plate J4882) ] /mag. mag e_RadBj25 Standard error on rBj number=16 A standard error value is only quoted here if the relevant parameter is based on the mean of two values [one from each of the two B_J_-band plates]. arcsec e_SuBrBjc Standard error on central B_J_ surface brightness number=16 A standard error value is only quoted here if the relevant parameter is based on the mean of two values [one from each of the two B_J_-band plates]. mag/arcsec2 e_SuBrBj25 Standard error mean surface brightness for mu(B_J_)<=25 number=16 A standard error value is only quoted here if the relevant parameter is based on the mean of two values [one from each of the two B_J_-band plates]. mag/arcsec2 e_Bjoverlap Standard error on overlapping B_J_ isophote number=16 A standard error value is only quoted here if the relevant parameter is based on the mean of two values [one from each of the two B_J_-band plates]. mag/arcsec2 U25 U_25 isophotal magnitude mag RadU25 Mean radius of mu(U)=25 isophote number=24 Mean radii= SQRT(A*B). arcsec SuBrUc Measured central U surface brightness mag/arcsec2 SuBrU25 Mean surface brightness for mu(U)<=25 mag/arcsec2 Uoverlap Brightest overlapping U isophote mag/arcsec2 UmagTot U_t_ total magnitude mag URn Sersic parameter n_U --- U0 Extrapolated Sersic central U surface brightness mag/arcsec2 r0U Sersic scale length r_0_U_ arcsec NU Number of U isophotes fitted --- R24 R_C_24 isophotal magnitude mag RadRc24 Mean radius of mu(R_C_)=24 isophote number=24 Mean radii= SQRT(A*B). arcsec SuBrRcc Measured central R_C_ surface brightness mag/arcsec2 SuBrRc24 Mean surface brightness for mu(R_C_)<=25 mag/arcsec2 Rcoverlap Brightest overlapping R isophote mag/arcsec2 RcTot R_C_t total magnitude mag RcRn Sersic parameter n_R_C_ --- Rc0 Extrapolated Sersic central R_C_ surface brightness mag/arcsec2 r0Rc Sersic scale length r_0_R_C_ arcsec NRc Number of R isophotes fitted --- Plate J4882 B_J_-band surface photometry (AppenB) Plate J9229 B_J_-band surface photometry (AppenB) Plate R2936 R_C_-band surface photometry (AppenB) Plate U9362 U-band surface photometry (AppenB) VPC VPC number --- Iso Isophotal surface brightness mag/arcsec+2 IntMag Integrated magnitude mag Radius Radius arcsec oFlag Overlap flag number=1 'o' if isophote overlaps with that of another image or images ' ' if isophote does not overlap any another image --- cFlag Cut flag number=2 'c' if isophote cut by edge of scan area ' ' if isophote not cut by edge of scan area --- Eps Ellipticity number=3 Ellipticity = 1-(B/A) where A & B are the major & minor diameters respectively --- PA Position angle number=4 Position angle = that of the major axis measured from the meridian through East deg Summary catalogue (AppenE) VPC VPC name ---- n_VPC *: object saturated in B_J_ --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec VCC VCC (Binggeli et al., 1985AJ.....90.1681B) number --- n_VCC Note on VCC number=1 B: background P: possible member M: member --- MType Morphological type number=2 E: elliptical S: spiral S0: lenticular I: irregular BCD: blue compact dwarf pre: pre-merger pec: peculiar Object that defied classification being assigned "?" --- r_MType Reference for Mtype number=3 1: VCC (Binggeli et al., 1985AJ.....90.1681B) 2: this work --- BJ25 Apparent B_J_ magnitude to the 25.0mag/arcsec^2^ isophote mag r_BJ25 Reference for BJ25 number=4 The value of BJ25 is the mean of two values independently derived from Plates J4882 and J9229, except when r_BJ25 not empty. 1: de Vaucouleurs & Pence (1979ApJS...40..425D), table2 2: de Vaucouleurs & Pence (1979ApJS...40..425D), table4 3: Binggeli et al. (1984AJ.....89...64B) 4: Binggeli et al. (1985AJ.....90.1681B) 5: Karachentsev & Karachentseva (1982PAZh....8..198K) 6: Mean of the sources 1 and 4 7: Mean of the sources 2 and 4 8: Mean of the sources 4 and 5 9: this work when an estimate was made by the authors by eye --- e_BJ25 rms uncertainty on BJ25 mag n_BJ25 R (reliable) or U (unreliable) from the VCC --- BjTot Total extrapolated magnitude mag BTot Transformed Bt (total extrapolated) magnitude mag n B_J_ band Sersic profile shape parameter --- mu0 B_J_ band Sersic extrapolated central surface surface brightness /mag.arcsec^-2^ --- r0 B_J_ band Sersic scale length parameter --- U-Bj U-B_J_ equal-area colour number=5 U-B_J_ equal-area colour if relevant VPC photometry unsaturated and not heavily merged (estimated mean error of ~0.2mag), or (U-0.65B-0.35V)_T_ from the RC3 whenever possible if VPC photometry saturated mag Bj-Rc (B_J_-R_C_) equal-area colour mag HRV Heliocentric radial velocity km/s r_HRV Reference for HRV number=6 1: Karachentsev & Karachentseva (1982PAZh....8..198K) 2: Karachentsev et al. (1983PAZh....9..387K) 3: Binggeli et al. (1985AJ.....90.1681B) 4: Rhee & Katgert (1988A&AS...72..243R) 5: de Vaucouleurs et al. (1991, Cat. <VII/155>), RC3 6: Binggeli et al. (1993A&AS...98..275B) 7: Drinkwater et al. (1996, Cat. <J/MNRAS/279/595>) --- sumcat1.tex LaTeX version of Part1 of sumcat.dat sumcat2.tex LaTeX version of Part2 of sumcat.dat sumcat3.tex LaTeX version of Part3 of sumcat.dat sumcat4.tex LaTeX version of Part4 of sumcat.dat sumcat1.ps PostScript version of Part1 of sumcat.dat sumcat2.ps PostScript version of Part2 of sumcat.dat sumcat3.ps PostScript version of Part3 of sumcat.dat sumcat4.ps PostScript version of Part4 of sumcat.dat Chris Young BAO 1998 May 27 Christopher Ke-shih Young <cky@vega.bac.pku.edu.cn> J_A+AS_127_367.xml A list of new nearby dwarf galaxy candidates J/A+AS/127/409 J/A+AS/127/409 New nearby dwarf galaxy candidates list A list of new nearby dwarf galaxy candidates V E Karachentseva I D Karachentsev Astron. Astrophys. Suppl. Ser. 127 409 1998 1998A&AS..127..409K Galaxies, nearby Morphology Radial velocities galaxies: distances and redshifts surveys To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg & Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a>0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.
List of new Local Volume dwarf candidates Other candidates selected in the visual search and rejected RAh Right ascension (J1950.0) h RAm Right ascension (J1950.0) min RAs Right ascension (J1950.0) s DE- Declination sign --- DEd Declination (J1950.0) deg DEm Declination (J1950.0) arcmin DEs Declination (J1950.0) arcsec MajAxis Diameter of major axis mm u_MajAxis Uncertainty flag on MajAxis --- MinAxis Diameter of minor axis mm u_MinAxis Uncertainty flag on MinAxis --- Type Type of the galaxy --- SB Surface brightness number=1 H: high L: low VL: very low EL: extremely low --- Id Identifications number=2 AM: Arp & Madore (1987, Cat. <VII/170>) FG: Feitzinger & Galinski (1985A&AS...61..503F) K: Karachentseva (1968SoByu..39...61K, 1972SoSAO...7....1K, 1973SoSAO...8....3K) BK: Borngen & Karachentseva (1985AN....306..301B) DDO: van den Bergh (1966, Cat. <VII/21>) UGC, UGCA: Nilson, 1973, Cat. <VII/26>, 1974UppOR...5.....N) F: Schombert et al. (1992AJ....103.1107S) VCC: Binggeli et al. (1985AJ.....90.1681B) MCG: Vorontsov-Velyaminov et al. (1962-1968, Cat. <VII/62>) --- HRV Heliocentric radial velocity km/s Patricia Bauer CDS 1997 Jun 03 Igor D. Karachentsev <ikar@luna.sao.ru> J_A+AS_127_409.xml Fundamental parameters of the highly reddened young open clusters Westerlund 1 and 2 J/A+AS/127/423 J/A+AS/127/423 VI photometry of Westerlund 1 and 2 Fundamental parameters of the highly reddened young open clusters Westerlund 1 and 2 A E Piatti E Bica J J Claria Astron. Astrophys. Suppl. Ser. 127 423 1998 1998A&AS..127..423P Clusters, open Photometry, CCD Hertzsprung-Russell (HR diagram) open clusters and associations: general open clusters and associations: individual (Westerlund 1, Westerlund 2) We have carried out CCD observations of stars in the region of the open cluster Westerlund 1 through the V and I passbands. The direct images were obtained with the 24-inch telescope of the University of Toronto Southern Observatory situated at Las Campanas Observatory, Chile. After cross-correlating all independent V, (V-I) tables we have obtained a improved set of colour and magnitude values as compared to those based on a single measure.
Westerlund 1 C 1644-457 16 48.2 -45 50 Westerlund 2 C 1022-575 10 23.9 -57 45
Photometric data ID Star number --- Xpos X coordinate number=1 X and Y coordinates increase toward the north and west, respectively. pix Ypos Y coordinate number=1 X and Y coordinates increase toward the north and west, respectively. pix Vmag V magnitude mag e_Vmag V magnitude error mag V-I V-I colour mag e_V-I V-I colour error mag o_Vmag Number of measurements --- Patricia Bauer CDS 1997 Jun 02 Andres Piatti <andres@oac.uncor.edu> J_A+AS_127_423.xml Optical photometric monitoring of gamma-ray loud blazars. II. Observations from November 1995 to June 1996 J/A+AS/127/445 J/A+AS/127/445 Gamma-ray loud blazars optical monitoring. II. Optical photometric monitoring of gamma-ray loud blazars. II. Observations from November 1995 to June 1996 C M Raiteri G Ghisellini M Villata G De Francesco L Lanteri M Chiaberge A Peila G Antico Astron. Astrophys. Suppl. Ser. 127 445 1998 1998A&AS..127..445R J/A+AS/121/119 : Gamma-ray loud blazars optical monitoring. I. (Villata+ 1997) BL Lac objects Photometry QSOs BL Lacertae objects: general galaxies: active quasars: general New data from the optical monitoring of gamma-ray loud blazars at the Torino Astronomical Observatory are presented.
Observations dates for tab2-21 data Name Blazar designation --- Band Band --- Obs1 Date of the beginning of observations "DD/MM/YY" Obs2 Date of the end of observations "DD/MM/YY" magMin Minimum magnitude in Band mag magMax Maximum magnitude in Band mag Nframes Number of frames --- RVB photometry Name QSO name --- Band Band --- magl Label of mag column number=1 B-B_A: B magnitude of the source minus the B magnitude of star A B-B_B: B magnitude of the source minus the B magnitude of star B R-R_A: R magnitude of the source minus the R magnitude of star A R-R_B: R magnitude of the source minus the R magnitude of star B R-R_D: R magnitude of the source minus the R magnitude of star D V-V_A: V magnitude of the source minus the V magnitude of star A V-V_B: V magnitude of the source minus the V magnitude of star B --- HJD Heliocentric Julian date d mag Magnitude or differential magnitude mag e_mag rms uncertainty on mag mag Patricia Bauer CDS 1997 Jun 26 Claudia M. Raiteri <raiteri@otoax3.to.astro.it> J_A+AS_127_445.xml Extragalactic Large-Scale Structures behind the Southern Milky Way. II. Redshifts Obtained at the SAAO in the Crux region J/A+AS/127/463 J/A+AS/127/463 Crux region redshifts Extragalactic Large-Scale Structures behind the Southern Milky Way. II. Redshifts Obtained at the SAAO in the Crux region A P Fairall P A Woudt R C Kraan-Korteweg Astron. Astrophys. Suppl. Ser. 127 463 1998 1998A&AS..127..463F VII/34 : ESO/Uppsala Survey of the ESO(B) Atlas (Lauberts 1982) J/A+A/297/617 : Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995) Woudt and Kraan-Korteweg, 1998, A Catalogue of 3760 Galaxies in the Zone of Avoidance in the Crux region (in press) Kraan-Korteweg, 1998, A Catalogue of 3279 Galaxies in the Zone of Avoidance in the Hydra/Antlia Extension (in press) Clusters, galaxy Radial velocities Redshifts galaxies: clusters: general galaxies: distances and redshifts large-scale structure of universe In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D>0.2' were identified in the Crux region (287{deg}<~l<~318{deg}, |b|<~10{deg}, Woudt & Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_<~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. <J/A+A/297/617>), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0<=v<=6000km/s (Fairall & Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000<=v<=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.
Redshifts of galaxies in the ZOA obtained at the SAAO Redshifts of galaxies in the ZOA (Hydra-Antlia region) obtained at the SAAO WKK Identification of the galaxy in the Catalogues of Woudt and Kraan-Korteweg, 1998 number=1 In table1.dat, Name as in "A Catalogue of 3760 Galaxies in the Zone of Avoidance in the Crux region (Woudt & Kraan-Korteweg, 1998, in press) In table2.dat, Name as in "A Catalogue of 3279 Galaxies in the Zone of Avoidance in the Hydra/Antlia Extension (Kraan-Korteweg, 1998, in press) --- ESO Identification in Lauberts Catalogue (1982, Cat. <VII/34>) --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg MajAxis Major axis arcsec MinAxis Minor axis arcsec Bmag B magnitude estimated from the IIIaJ ESO/SRC film copy mag MType Morphological type --- HVa Heliocentric velocity from absorption line features km/s e_HVa Error to absorption velocity km/s n_HVa Note on HVa (]: tentative redshift) --- HVe Heliocentric velocity from emission line features km/s e_HVe Error of emission velocity km/s n_HVe Note on HVe (]: tentative redshift) --- Code1 Code for identified emission line number=2 1: [OII] 3727 2: Hgamma 4340 3: Hbeta 4861 4: [OIII] 4959 5: [OIII] 5007 6: Halpha 6563 7: [NII] 6584 --- u_Code1 ":" : identification is tentative --- Code2 Code for identified emission line number=2 1: [OII] 3727 2: Hgamma 4340 3: Hbeta 4861 4: [OIII] 4959 5: [OIII] 5007 6: Halpha 6563 7: [NII] 6584 --- u_Code2 ":" : identification is tentative --- Code3 Code for identified emission line number=2 1: [OII] 3727 2: Hgamma 4340 3: Hbeta 4861 4: [OIII] 4959 5: [OIII] 5007 6: Halpha 6563 7: [NII] 6584 --- u_Code3 ":" : identification is tentative --- Code4 Code for identified emission line number=2 1: [OII] 3727 2: Hgamma 4340 3: Hbeta 4861 4: [OIII] 4959 5: [OIII] 5007 6: Halpha 6563 7: [NII] 6584 --- Code5 Code for identified emission line number=2 1: [OII] 3727 2: Hgamma 4340 3: Hbeta 4861 4: [OIII] 4959 5: [OIII] 5007 6: Halpha 6563 7: [NII] 6584 --- Code6 Code for identified emission line number=2 1: [OII] 3727 2: Hgamma 4340 3: Hbeta 4861 4: [OIII] 4959 5: [OIII] 5007 6: Halpha 6563 7: [NII] 6584 --- Rem Code for remarks to table 1 number=3 *: Redshifts are also available in the literature #: These galaxies are not in our search area, but do lie in the ``Zone of Avoidance''. The diameters and type are from Lauberts 1982 1: WKK 150: The redshift measured at the SAAO for this galaxy is in disagreement with the value quoted in the literature (v=8948+/-40km/s, Fisher et al., 1995, Cat. <VII/185>). It might be due to an identification error; a neighbouring galaxy (WKK 158) was found to be in good agreement with the value quoted in the literature. 2: The redshifts for these galaxies are tentative only, but confirmed by independent redshifts from the literature 3: KK1196: The redshift measured at the SAAO for this galaxy is in slight disagreement with the value quoted in the literature (v=2411km/s, Huchtmeier and Richter, 1989, The General Catalogue of HI-Observations og Galaxies. New York: Springer-Verlag) 4: L216- 5: The redshift measured at the SAAO for this galaxy is in slight disagreement with the value quoted in the literature (v=6350km/s, Visvanathan and v.d. Bergh, 1992AJ....103.1057V) Gal: Identification as galaxy questionable, spectra indicates a galactic origin PN: WKK P8: This object was classified as a possible PN, but was not listed in PNe list of Acker (1992, Cat. <V/84>). It has now been confirmed as a PN Sy2: These four galaxies have been classified as Seyfert 2 --- Galaxies observed at the SAAO without reliable redshift WKK Identification of the galaxy in the catalogue of Woudt and Kraan-Korteweg, 1998 number=1 Name as in "A Catalogue of 3760 Galaxies in the Zone of Avoidance in the Crux region (Woudt and Kraan-Korteweg, 1998, in press) --- ESO Identification in Lauberts Catalogue (1982, Cat. <VII/34>) --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg MajAxis Major axis arcsec MinAxis Minor axis arcsec Bmag B magnitude estimated from the IIIaJ ESO/SRC film copy mag MType Morphological type --- Rem Remark describing reason for non-detection of velocity --- Galaxies in our survey region with velocities from the literature WKK Identification of the galaxy as in A Catalogue of 3760 Galaxies in the Zone of Avoidance in the Crux region (Woudt and Kraan-Korteweg, 1998, in press) --- ESO Identification in Lauberts Catalogue (1982, Cat. <VII/34>) --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg MajAxis Major axis arcsec MinAxis Minor axis arcsec Bmag B magnitude estimated from the IIIaJ ESO/SRC film copy mag MType Morphological type --- HV Heliocentric velocity km/s e_HV Error to heliocentric velocity km/s r_HV Code for source of the velocity number=1 1: Dressler 1991, Cat. <J/ApJS/75/241> The supergalactic plane redshift survey 2: Strauss et al., 1992ApJS...83...29S, A redshift survey of IRAS galaxies 3: Visvanathan and v.d. Bergh, 1992AJ....103.1057V, Luminous spiral galaxies in the direction of the Great Attractor 4: Fairall, 1983MNRAS.203...47F, Spectroscopic survey of southern compact and bright-nucleus galaxies 5: Fisher et al. 1995, Cat. <VII/185>, The IRAS 1.2 Jy Survey 6: Fairall 1996, The Southern Redshift Catalogue (See Cat. <VII/142>) -------------------------------------------------------------------------------- Acknowledgements: Tony Fairall <fairall@uctvms.uct.ac.za> --- Patricia Bauer CDS 1998 Jan 05 J_A+AS_127_463.xml A statistical study of the spectra of very luminous IRAS galaxies. I. Data J/A+AS/127/521 J/A+AS/127/521 Very luminous IRAS galaxies spectra. A statistical study of the spectra of very luminous IRAS galaxies. I. Data H Wu Z L Zou X Y Xia Z G Deng Astron. Astrophys. Suppl. Ser. 127 521 1998 1998A&AS..127..521W II/174 : IRAS 2Jy Redshift Survey Data File Atlases Galaxies, IR Galaxies, spectra Redshifts galaxies: distances and redshifts galaxies: general galaxies: statistics infrared: galaxies This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)>=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag<=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. <II/174>). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.
Infrared luminosities, magnitudes, redshifts IRAS Source name --- n_IRAS Note on name number=1 *: sources also observed by Kim et al. (1995ApJS...98..129K) ): sources in brackets out of the complete sample (See paper). --- log(L_IR_) Infrared luminosity (H0=50km/s/Mpc,q0=0.5) [solLum] mag Magnitude from 2Jy catalog (Strauss, 1992ApJS...83...29S, Cat. <II/174>) mag z redshift from 2Jy catalog --- Source names, coordinates, observation parameters IRAS Source name --- m_IRAS Components name --- Name Other name of IRAS sources --- RAh Right Ascension (1950.0) h RAm Right Ascension (1950.0) min RAs Right Ascension (1950.0) s DE- Declination sign (1950) --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec OBSdate Date of observation "DD/MM/YY" OBSh B.T. Time of observation h OBSm B.T. Time of observation min OBSs B.T. Time of observation s Exp Exposure time s Airmass Airmass --- Slit Slit width arcsec PA Position angle deg Emission line ratios IRAS Source name --- m_IRAS Components name --- [OII]3727 Relative flux of emission line [OII]3727 number=1 Halpha = 1 --- u_[OII]3727 Uncertainty flag on [OII]3727 number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- Hb4861 Relative flux of emission line Hb4861 number=1 Halpha = 1 --- u_Hb4861 Uncertainty flag on Hb4861 number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- [OIII]5007 Relative flux of emission line [OIII]5007 number=1 Halpha = 1 --- u_[OIII]5007 Uncertainty flag on [OIII]5007 number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- HeI5876 Relative flux of emission line HeI5876 number=1 Halpha = 1 --- u_HeI5876 Uncertainty flag on HeI5876 number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- [OI]6300 Relative flux of emission line [OI]6300 number=1 Halpha = 1 --- u_[OI]6300 Uncertainty flag on [OI]6300 number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- [NII]6563 Relative flux of emission line [NII]6563 number=1 Halpha = 1 --- u_[NII]6563 Uncertainty flag on [NII]6563 number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- [SII]6716 Relative flux of emission line [SII]6716 number=1 Halpha = 1 --- u_[SII]6716 Uncertainty flag on [SII]6716 number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- [SII]6731 Relative flux of emission line [SII]6731 number=1 Halpha = 1 --- u_[SII]6731 Uncertainty flag on [SII]6731 number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- [SII]sum Relative flux of emission line [SII]sum number=1 Halpha = 1 --- u_[SII]sum Uncertainty flag on [SII]sum number=2 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- Fluxes, Equivalence Widths, Continuum fluxes IRAS Source name --- m_IRAS Components name --- z Measured redshift from observed spectra --- F(Ha) Observed flux of H{alpha} emission line 10+7W/m2/m u_F(Ha) Uncertainty flag on F(Ha) number=1 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- EW(Ha) Equivalent width of H{alpha} emission line 0.1m u_EW(Ha) Uncertainty flag on EW(Ha) number=1 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- EW(NaID) Equivalent width of NaID absorption 0.1m u_EW(NaID) Uncertainty flag on EW(NaID) number=1 : flux value uncertainty ~+/-30% ; flux value uncertainty ~+/-50% --- EW(Hb) Equivalent width of underlying stellar H{beta} absorption 0.1m C4861 Observed flux of Continuum at 4861A 10+7W/m2/m C6563 Observed flux of Continuum at 6563A 10+7W/m2/m tables.tex LaTeX version of tables 2, 3, and 4 Patricia Bauer CDS 1997 Jun 23 Hong Wu <wu@qso.bao.ac.cn> UNKNOWN UNKNOWN IRAS 05084+7936 misprint for IRAS 05083+7936. Correction made on 03-Apr-1998 J_A+AS_127_521.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest XVI: S V spectral lines J/A+AS/127/543 J/A+AS/127/543 Stark broadening of S V lines Stark broadening of spectral lines of multicharged ions of astrophysical interest XVI: S V spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 127 543 1998 1998A&AS..127..543D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines Atomic physics atomic data line: profiles Using a semiclassical approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 34 S V multiplets for perturber densities 10^17^-10^21^cm^-3^ and temperatures T=20000-1000000K. For lower perturber densities, the obtained results are linear with perturber density.
Stark broadening parameters due to e-, p- and He III-impacts for S V N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for N_V_>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for N_V_>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ (4) --- WHe++ FWHM for He II-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ (4) --- dHe++ shift for He II-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1997 May 30 Milan Dimitrijevic <mdimitrijevic@aob.aob.bg.ac.yu> J_A+AS_127_543.xml Photometric study of the open cluster NGC 2323 J/A+AS/128/131 J/A+AS/128/131 UBV photometry of NGC 2323 Photometric study of the open cluster NGC 2323 J J Claria A E Piatti E Lapasset Astron. Astrophys. Suppl. Ser. 128 131 1998 1998A&AS..128..131C Clusters, open Cross identifications Photometry, UBV Hertzsprung-Russell (HR diagram) open clusters and associations: general open clusters and associations: individual (NGC 2323) UBV and DDO photoelectric photometry in the field of the open cluster NGC 2323 is presented. The analysis yields 109 probable members; one of them being a red giant, and 3 possible members. The basic cluster parameters are derived. NGC 2323 appears not to be physically connected to the CMa OB1 association.
UBV data Star Star number --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag U-B U-B colour index mag e_U-B rms uncertainty on U-B mag o_Vmag Number of measurements --- Remarks Remarks number=1 a: Double star, both components measured together. b: Red giant candidate; membership is based on radial velocities and combined BV-DDO data (see Table 5). --- *Identifications, and positions Star Star number --- ID1 ID from Cuffey, 1941ApJ....94...55C --- ID2 ID from Becker et al., 1976AUBas.C......1B --- ID3 ID from Hoag et al., 1961PUSNO..17..343H (pe) --- ID4 ID from Hoag et al., 1961PUSNO..17..343H (pg) --- ID5 ID from Purgathorfer, 1964AnWie..26...37P --- ID6 ID from Mostafa et al., 1983JASEg...5...23M --- RAh Right Ascension J2000 (hours) number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. h RAm Right Ascension J2000 (minutes) number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. min RAs Right Ascension J2000 (seconds) number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. s DE- Declination J2000 (sign) number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. --- DEd Declination J2000 (degrees) number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. deg DEm Declination J2000 (minutes) number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. arcmin DEs Declination J2000 (seconds) number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. arcsec GSC Designation in GSC <I/220> number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. --- Rem Other names and Remarks number=1 The last columns are not in the original publication, but were supplied by B. Skiff (bas@lowell.Lowell.Edu). Positions are generally originated from GSC (Cat. <I/220>), unless stated in the "Rem" column ("A1" stands for Monnet's "USNO-A1.0 Catalogue", see Cat. <I/243>). GSC names are supplied, and names in some other catalogues are supplied in the Rem column. --- Patricia Bauer CDS 1997 Nov 24 Juan Claria <claria@oac.uncor.edu> UNKNOWN UNKNOWN * 24-Nov-1977: Tables from Juan Claria <claria@oac.uncor.edu> * 14-Aug-1998: Position, GSC identifications and remarks in table2 supplied by Brian Skiff (bas@lowell.Lowell.Edu) J_A+AS_128_131.xml Four colour photometry of binary systems. III. The early-type binary system CR Cassiopeiae J/A+AS/128/139 J/A+AS/128/139 ubvy photometry of CR Cas Four colour photometry of binary systems. III. The early-type binary system CR Cassiopeiae R Clement J Fabregat Astron. Astrophys. Suppl. Ser. 128 139 1998 1998A&AS..128..139C J/A+AS/123/1 : uvbyBeta photometry of ZZ UMa (Clement+ 1997) J/A+AS/123/59 : uvby photometry of BH Vir (Clement+ 1997) Binaries, eclipsing Photometry, uvby binaries: eclipsing stars: early-type stars: fundamental parameters stars: individual (CR Cas) The table contains the differential magnitudes of CR Cas respect to comparison star SAO35044 indicating the time (Julian Date) a nd magnitudes in Stroemgren filters u, v, b, y
CR Cas 23 04 52.0 +59 33 57
Differential magnitudes for CR Cas HJD Heliocentric Julian date d umag u magnitude mag vmag v magnitude mag bmag b magnitude mag ymag y magnitude mag table4.tex LaTeX version of table4 Rosa Clement GACE Patricia Bauer CDS 1997 Jun 24 Rosa Clement (GACE) clement@deneb.matapl.uv.es J_A+AS_128_139.xml The revised GB/GB2 sample of extragalactic radio sources J/A+AS/128/153 J/A+AS/128/153 Revised GB/GB2 sample of radio sources The revised GB/GB2 sample of extragalactic radio sources J Machalski Astron. Astrophys. Suppl. Ser. 128 153 1998 1998A&AS..128..153M VIII/25 : 6C Survey of radio sources - VI. (Hales+ 1993) VIII/42 : Texas Survey of radio sources at 365MHz (Douglas+ 1996) VIII/36 : The Second Bologna Survey (Colla+ 1970-74) VIII/17 : THE 1.4GHz NORTHERN SKY CATALOG J/ApJS/75/801 : MGIV (Fourth MIT-Green Bank) 5GHz Survey (Griffith+ 1991) VIII/40 : GB6 catalog of radio sources (Gregory+ 1996) Binaries, eclipsing Photometry, uvby galaxies: active quasars: general radio continuum: galaxies radio continuum: general surveys The revised sample of 373 extragalactic radio sources brighter than 0.2 Jy at 1.4GHz is presented. These sources, selected from the finding Green Bank surveys, were mapped at 1465 MHz using the VLA at different configurations. The biases introduced into the original GB (Maslowski, 1972AcA....22..227M) and GB2 (Machalski, 1978AcA....28..367M) catalogues by confusion as well as partial resolution by the VLA at its A-configuration, are eliminated. In effect, a number of sources have been excluded, and a few other are included into the revised sample. Now the sample is about 99, 97 and 95 per cent complete for sources with S_1.4_>=0.55Jy, 0.25Jy<=S_1.4_<0.55Jy, and 0.2Jy<=S_1.4_<0.25Jy, respectively. Table 3 gives the compilation of the radio, optical, and X-ray data available for the sample sources.
Radio, optical and X-ray data for 373 sources IAU IAU-format source name, based on 1950 position --- Cat1 Presence in 151 MHz: 6CII, III, VI number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Cat2 Presence in 178 MHz:4C number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Cat3 Presence in 365-MHz: Texas number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Cat4 Presence in 408 MHz: B2(1) --- Cat5 Presence in B3 number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Cat6 Presence in 750 and 1400 MHz: NRAO number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Cat7 Presence in 966 MHz: Jodrell Bank number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Cat8 Presence in 1400 MHz: 83GB number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Cat9 Presence in 4830 MHz: MGII, MGIV number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Cat10 Presence in 4850 MHz: GB6 number=1 *: presence n: absence c: flux contaminated by confusing source or sources r: source resolved, flux underestimated Cat1: 151 MHz: 6CII, III, VI (Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> and references therein) Cat2: 178 MHz:4C (Pilkington & Scott 1965MmRAS..69..183P; Gower et al. 1967MmRAS..71...49G) Cat3: 365-MHz: Texas (Douglas et al. 1980PAUTx..17....1D, Cat. <VIII/42>) Cat4: 408 MHz: B2 (Colla et al., 1973A&AS...11..291C, Cat. <VIII/36> Cat5: B3 (Ficarra et al. 1985A&AS...59..255F, Cat. <VIII/37>) Cat6: 750 and 1400 MHz: NRAO (Pauliny-Toth et al. 1966ApJS...13...65P) Cat7: 966 MHz: Jodrell Bank (Cohen et al. 1977MmRAS..84....1C; Porcas et al. 1980MNRAS.191..607P), Cat8: 1400 MHz: 83GB (Condon & Broderick 1985AJ.....90.2540C, White & Becker 1992ApJS...79..331W, Cat. <VIII/17>) Cat9: 4830 MHz: MGII, MGIV (Langston et al. 1990ApJS...72..621L, Griffith et al. 1991, Cat. <J/ApJS/75/801> respectively) Cat10: 4850 MHz: GB6 (Gregory et al. 1996ApJS..103..427G, Cat. <VIII/40>) --- Part Subsamples number=2 1: the source belongs to Subsample 1 complete to S>=0.55Jy in the sky area of 0.4414 sr 2: the source belongs to Subsample 2 complete with 0.25Jy<=S<0.55Jy in the sky area of 0.0906 sr 3: the source belongs to Subsample 3 complete with 0.20Jy<=S<0.25Jy in the area of 0.0550 sr 1,2: denotes sources with S>=0.25 Jy in the area of 0.0906 sr 2,3: denotes sources with 0.20Jy<=S<0.55Jy in the area of 0.0550 sr --- S1.4GHz Weighted mean 1.4-GHz flux density mJy e_S1.4GHz rms uncertainty on S1.4GHz mJy n_S1.4GHz Value in [] --- sigS1.4GHz Standard deviation of variable flux mJy SI Slope of the fitted spectrum at 1.4 GHz number=3 The slope is the derivative of a function y=a+bx+cx^2^ or y=a+bx+d\c{dot}exp(+/-x). If no function could be fitted to the spectral data (generally for variable sources), a crude slope at 1.4 GHz is given followed by u_SI=')' --- e_SI rms uncertainty on SI --- u_SI See Note number=3 The slope is the derivative of a function y=a+bx+cx^2^ or y=a+bx+d\c{dot}exp(+/-x). If no function could be fitted to the spectral data (generally for variable sources), a crude slope at 1.4 GHz is given followed by u_SI=')' --- radType Type of radio spectrum --- radMorph Radio morphology number=4 FRI: edge-darkened double FRII: edge-brightened double C: compact, unresolved with the VLA C(1s): core-dominated compact with one-sided extended emission C(2s): core-dominated compact with two-sided extended emission cc: appended to the type denotes that a compact core has been detected CSS: compact steep-spectrum Di: diffuse emission --- l_LAS Limit flag on LAS --- LAS Largest angular size arcsec u_LAS ?: Unknown value --- map Code concerning the VLA maps available number=5 Code concerning the VLA maps available. '1.4' and sometimes '4.9' indicate observing frequency, and ABCP: VLA configuration used for observations ('P' means partially completed VLA in 1980). * denotes that no map is available, and the source is represented by fitted Gaussian components only. If the VLBI-scale structure has been observed in a compact source, this is indicated --- optType Optical type number=6 Optical type. GAL : galaxy confirmed spectroscopically and/or with an extended image (GAL) : possibly a galaxy GAL? : identification ambiguous QSO : quasar confirmed spectroscopically BL : BL Lac object RSO : red stellar object NSO : neutral stellar object (most of them are quasar candidates) BSO : blue stellar object (most of them are quasar candidates) RO : red object too faint to be recognized as stellar or extended. BO : blue object too faint to be recognized as stellar or extended. EF : 'empty field' source, an identification likely beyond the POSS limit. 'X' preceding the type indicates that an X-ray source coincides with the radio position --- z Redshift --- u_z ): Redshift estimated from the apparent magnitude and colour --- l_Rmag Limit flag on R magnitude --- Rmag R magnitude number=7 Two decimal digits precision indicate magnitudes measured with photoelectric or CCD photometry mag n_Rmag v: variable --- l_Bmag Limit flag on Bmag --- Bmag B magnitude number=7 Two decimal digits precision indicate magnitudes measured with photoelectric or CCD photometry mag n_Bmag v: variable --- n_Pos o: optical object position number=8 For double source without a radio core, the given position corresponds to a radio centroid --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Ref1 References to large-scale radio structure and VLA maps number=9 References to VLA maps 1 Antonucci (1985ApJS...59..499A) 2 Burns et al. (1983ApJ...271..575B) 3 Capetti et al. (1993A&AS...99..407C) 4 Condon (1983ApJS...53..459C) 5 Condon & Broderick (1988AJ.....96...30C) 6 de Ruiter et al. (1986A&AS...65..111D) 7 Fanti et al. (1986A&AS...65..145F) 8 Fanti et al. (1987A&AS...69...57F) 9 Ford et al. (1985ApJ...293..132F) 10 Gioia & Fabbiano (1987ApJS...63..771G) 11 Hummel et al. (1985A&AS...60..293H) 12 Leahy & Perley (1991AJ....102..537L) 13 Lonsdale et al. (1993ApJS...87...63L) 14 Machalski et al. (1982AJ.....87.1150M), Paper II 15 Machalski & Condon (1983AJ.....88..143M), Paper III 16 Machalski & Condon (1983AJ.....88.1591M), Paper IV 17 Machalski & Condon (1985AJ.....90....5M), Paper V 18 Machalski & Condon (1985AJ.....90..973M) 19 Machalski & Condon (1986AJ.....91..998M) 20 Maslowski & Kellermann (1988AJ.....95.1659M) 21 O'Donoghue et al. (1993ApJ...408..428O) 22 Owen & Puschell (1984AJ.....89..932O) 23 Parma et al. (1986A&AS...64..135P) 24 Perley et al. (1980AJ.....85..649P) 25 Perley (1982AJ.....87..859P) 26 Perley et al. (1982ApJ...255L..93P) 27 Reid et al. (1995A&AS..110..213R) 28 Vallee et al. (1981ApJ...250...66V) 29 Vallee & Wilson (1976Natur.259..451V) 30 van Albada & van der Hulst (1982A&A...115..263V) 31 Vigotti et al. (1989A&AS...36..237W) 32 4885-MHz map in Figure A1. (Appendix) References to VLBI maps. 40 Henstock et al. (1995, Cat. <J/ApJS/100/1>) 41 Morabito et al. (1986AJ.....91.1038M) 42 Pearson & Readhead (1988ApJ...328..114P) 43 Polatidis et al. (1995, Cat. <J/ApJS/98/1>) 44 Thakkar et al. (1995, Cat. <J/ApJS/98/33>) 45 Xu et al. (1995, Cat. <J/ApJS/99/297>) 46 Rioja et al. (1996, Proc. IAU Symp. No.175, p.122) 47 Fey et al. (1996ApJS..105..299F) References to photometry 50 Allington-Smith et al. (1982MNRAS.201..331A) 51 Laing et al. (1983MNRAS.204..151L) 52 Machalski & Wisniewski (1988MNRAS.231.1065M) 53 Machalski (1992AcA....42..335M) 54 Machalski & Magdziarz (1993A&AS..102..315M) 57 Sandage (1972ApJ...176...21S) of Pointed Observations 55 Machalski & LaFranca (1988IAUC.4573.....M) 56 Moles et al. (1985A&A...152..271M) 58 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 59 Netzer et al. (1996MNRAS.279..429N) 591 Hook et al. (1996MNRAS.282.1274H) References to redshift 60 Allington-Smith et al. (1988MNRAS.234.1091A) 61 Burbidge (1970ApJ...160L..33B) 62 Burbidge & Strittmatter (1972ApJ...172L..37B) 63 Djorgovski et al. (1990PASP..102..113D) 64 Grueff et al. (1980A&A....86...50G) 65 Grueff & Vigotti (1979A&AS...35..371G) 66 Henstock (1995, priv. info.) 67 Hewitt & Burbidge (1993ApJS...87..451H, Cat. <VII/158>) 68 Huchra et al. (1983ApJS...52...89H, Cat. <VII/193>) 69 Katgert-Merkelijn et al. (1980A&AS...40...91K) 70 Laing et al. (1983MNRAS.204..151L) 71 Lilly et al. (1985MNRAS.215...37L) 72 Machalski (1991AcA....41...39M) 73 Machalski & Engels (1994MNRAS.266L..69M) 74 Morganti et al. (1992MNRAS.254..546M) 75 Owen et al. (1988AJ.....95....1O) 76 Sandage et al. (1976ApJ...205..688S) 77 Sargent (1973ApJ...182L..13S) 78 Smith & Spinrad (1980PASP...92..553S) 79 Spinrad (1982PASP...94..397S) 80 Spinrad & Djorgovski (1984ApJ...285L..49S) 81 Spinrad et al. (1985ApJ...299L...7S) 82 Stickel & Kuehr (1994, Cat. <J/A+AS/105/67>) 83 Strittmatter et al. (1974ApJ...190..509S) 84 Strom et al. (1990A&A...227...19S) 85 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 86 Vigotti et al. (1989AJ.....98..419V) 87 Walsh et al. (1979MNRAS.189..667W) 88 Warner et al. (1983MNRAS.204.1279W) 89 Wilkinson et al. (1981MNRAS.196..669W) 90 Zwicky & Herzog (1963, See Cat. <VII/4>) 91 LaHulla et al. (1991A&AS...88..525L) 92 Vermeulen et al. (1996AJ....111.1013V) 93 Sanghera et al. (1995A&A...295..629S) 94 Maxfield et al. (1995PASP..107..369M) References to X-ray data X1 Crawford & Fabian (1996MNRAS.282.1483C) X2 ROSAT Catalogue (See e.g. Cat. <IX/11>) X3 Worrall & Wilkes (1990ApJ...360..396W) X4 Wilkes et al. 1994, Cat. <J/ApJS/92/53> X5 Machalski & Brandt (1996MNRAS.282.1305M) --- Ref2 References to VLBI- scale structure number=9 References to VLA maps 1 Antonucci (1985ApJS...59..499A) 2 Burns et al. (1983ApJ...271..575B) 3 Capetti et al. (1993A&AS...99..407C) 4 Condon (1983ApJS...53..459C) 5 Condon & Broderick (1988AJ.....96...30C) 6 de Ruiter et al. (1986A&AS...65..111D) 7 Fanti et al. (1986A&AS...65..145F) 8 Fanti et al. (1987A&AS...69...57F) 9 Ford et al. (1985ApJ...293..132F) 10 Gioia & Fabbiano (1987ApJS...63..771G) 11 Hummel et al. (1985A&AS...60..293H) 12 Leahy & Perley (1991AJ....102..537L) 13 Lonsdale et al. (1993ApJS...87...63L) 14 Machalski et al. (1982AJ.....87.1150M), Paper II 15 Machalski & Condon (1983AJ.....88..143M), Paper III 16 Machalski & Condon (1983AJ.....88.1591M), Paper IV 17 Machalski & Condon (1985AJ.....90....5M), Paper V 18 Machalski & Condon (1985AJ.....90..973M) 19 Machalski & Condon (1986AJ.....91..998M) 20 Maslowski & Kellermann (1988AJ.....95.1659M) 21 O'Donoghue et al. (1993ApJ...408..428O) 22 Owen & Puschell (1984AJ.....89..932O) 23 Parma et al. (1986A&AS...64..135P) 24 Perley et al. (1980AJ.....85..649P) 25 Perley (1982AJ.....87..859P) 26 Perley et al. (1982ApJ...255L..93P) 27 Reid et al. (1995A&AS..110..213R) 28 Vallee et al. (1981ApJ...250...66V) 29 Vallee & Wilson (1976Natur.259..451V) 30 van Albada & van der Hulst (1982A&A...115..263V) 31 Vigotti et al. (1989A&AS...36..237W) 32 4885-MHz map in Figure A1. (Appendix) References to VLBI maps. 40 Henstock et al. (1995, Cat. <J/ApJS/100/1>) 41 Morabito et al. (1986AJ.....91.1038M) 42 Pearson & Readhead (1988ApJ...328..114P) 43 Polatidis et al. (1995, Cat. <J/ApJS/98/1>) 44 Thakkar et al. (1995, Cat. <J/ApJS/98/33>) 45 Xu et al. (1995, Cat. <J/ApJS/99/297>) 46 Rioja et al. (1996, Proc. IAU Symp. No.175, p.122) 47 Fey et al. (1996ApJS..105..299F) References to photometry 50 Allington-Smith et al. (1982MNRAS.201..331A) 51 Laing et al. (1983MNRAS.204..151L) 52 Machalski & Wisniewski (1988MNRAS.231.1065M) 53 Machalski (1992AcA....42..335M) 54 Machalski & Magdziarz (1993A&AS..102..315M) 57 Sandage (1972ApJ...176...21S) of Pointed Observations 55 Machalski & LaFranca (1988IAUC.4573.....M) 56 Moles et al. (1985A&A...152..271M) 58 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 59 Netzer et al. (1996MNRAS.279..429N) 591 Hook et al. (1996MNRAS.282.1274H) References to redshift 60 Allington-Smith et al. (1988MNRAS.234.1091A) 61 Burbidge (1970ApJ...160L..33B) 62 Burbidge & Strittmatter (1972ApJ...172L..37B) 63 Djorgovski et al. (1990PASP..102..113D) 64 Grueff et al. (1980A&A....86...50G) 65 Grueff & Vigotti (1979A&AS...35..371G) 66 Henstock (1995, priv. info.) 67 Hewitt & Burbidge (1993ApJS...87..451H, Cat. <VII/158>) 68 Huchra et al. (1983ApJS...52...89H, Cat. <VII/193>) 69 Katgert-Merkelijn et al. (1980A&AS...40...91K) 70 Laing et al. (1983MNRAS.204..151L) 71 Lilly et al. (1985MNRAS.215...37L) 72 Machalski (1991AcA....41...39M) 73 Machalski & Engels (1994MNRAS.266L..69M) 74 Morganti et al. (1992MNRAS.254..546M) 75 Owen et al. (1988AJ.....95....1O) 76 Sandage et al. (1976ApJ...205..688S) 77 Sargent (1973ApJ...182L..13S) 78 Smith & Spinrad (1980PASP...92..553S) 79 Spinrad (1982PASP...94..397S) 80 Spinrad & Djorgovski (1984ApJ...285L..49S) 81 Spinrad et al. (1985ApJ...299L...7S) 82 Stickel & Kuehr (1994, Cat. <J/A+AS/105/67>) 83 Strittmatter et al. (1974ApJ...190..509S) 84 Strom et al. (1990A&A...227...19S) 85 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 86 Vigotti et al. (1989AJ.....98..419V) 87 Walsh et al. (1979MNRAS.189..667W) 88 Warner et al. (1983MNRAS.204.1279W) 89 Wilkinson et al. (1981MNRAS.196..669W) 90 Zwicky & Herzog (1963, See Cat. <VII/4>) 91 LaHulla et al. (1991A&AS...88..525L) 92 Vermeulen et al. (1996AJ....111.1013V) 93 Sanghera et al. (1995A&A...295..629S) 94 Maxfield et al. (1995PASP..107..369M) References to X-ray data X1 Crawford & Fabian (1996MNRAS.282.1483C) X2 ROSAT Catalogue (See e.g. Cat. <IX/11>) X3 Worrall & Wilkes (1990ApJ...360..396W) X4 Wilkes et al. 1994, Cat. <J/ApJS/92/53> X5 Machalski & Brandt (1996MNRAS.282.1305M) --- Ref3 References to photometry number=9 References to VLA maps 1 Antonucci (1985ApJS...59..499A) 2 Burns et al. (1983ApJ...271..575B) 3 Capetti et al. (1993A&AS...99..407C) 4 Condon (1983ApJS...53..459C) 5 Condon & Broderick (1988AJ.....96...30C) 6 de Ruiter et al. (1986A&AS...65..111D) 7 Fanti et al. (1986A&AS...65..145F) 8 Fanti et al. (1987A&AS...69...57F) 9 Ford et al. (1985ApJ...293..132F) 10 Gioia & Fabbiano (1987ApJS...63..771G) 11 Hummel et al. (1985A&AS...60..293H) 12 Leahy & Perley (1991AJ....102..537L) 13 Lonsdale et al. (1993ApJS...87...63L) 14 Machalski et al. (1982AJ.....87.1150M), Paper II 15 Machalski & Condon (1983AJ.....88..143M), Paper III 16 Machalski & Condon (1983AJ.....88.1591M), Paper IV 17 Machalski & Condon (1985AJ.....90....5M), Paper V 18 Machalski & Condon (1985AJ.....90..973M) 19 Machalski & Condon (1986AJ.....91..998M) 20 Maslowski & Kellermann (1988AJ.....95.1659M) 21 O'Donoghue et al. (1993ApJ...408..428O) 22 Owen & Puschell (1984AJ.....89..932O) 23 Parma et al. (1986A&AS...64..135P) 24 Perley et al. (1980AJ.....85..649P) 25 Perley (1982AJ.....87..859P) 26 Perley et al. (1982ApJ...255L..93P) 27 Reid et al. (1995A&AS..110..213R) 28 Vallee et al. (1981ApJ...250...66V) 29 Vallee & Wilson (1976Natur.259..451V) 30 van Albada & van der Hulst (1982A&A...115..263V) 31 Vigotti et al. (1989A&AS...36..237W) 32 4885-MHz map in Figure A1. (Appendix) References to VLBI maps. 40 Henstock et al. (1995, Cat. <J/ApJS/100/1>) 41 Morabito et al. (1986AJ.....91.1038M) 42 Pearson & Readhead (1988ApJ...328..114P) 43 Polatidis et al. (1995, Cat. <J/ApJS/98/1>) 44 Thakkar et al. (1995, Cat. <J/ApJS/98/33>) 45 Xu et al. (1995, Cat. <J/ApJS/99/297>) 46 Rioja et al. (1996, Proc. IAU Symp. No.175, p.122) 47 Fey et al. (1996ApJS..105..299F) References to photometry 50 Allington-Smith et al. (1982MNRAS.201..331A) 51 Laing et al. (1983MNRAS.204..151L) 52 Machalski & Wisniewski (1988MNRAS.231.1065M) 53 Machalski (1992AcA....42..335M) 54 Machalski & Magdziarz (1993A&AS..102..315M) 57 Sandage (1972ApJ...176...21S) of Pointed Observations 55 Machalski & LaFranca (1988IAUC.4573.....M) 56 Moles et al. (1985A&A...152..271M) 58 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 59 Netzer et al. (1996MNRAS.279..429N) 591 Hook et al. (1996MNRAS.282.1274H) References to redshift 60 Allington-Smith et al. (1988MNRAS.234.1091A) 61 Burbidge (1970ApJ...160L..33B) 62 Burbidge & Strittmatter (1972ApJ...172L..37B) 63 Djorgovski et al. (1990PASP..102..113D) 64 Grueff et al. (1980A&A....86...50G) 65 Grueff & Vigotti (1979A&AS...35..371G) 66 Henstock (1995, priv. info.) 67 Hewitt & Burbidge (1993ApJS...87..451H, Cat. <VII/158>) 68 Huchra et al. (1983ApJS...52...89H, Cat. <VII/193>) 69 Katgert-Merkelijn et al. (1980A&AS...40...91K) 70 Laing et al. (1983MNRAS.204..151L) 71 Lilly et al. (1985MNRAS.215...37L) 72 Machalski (1991AcA....41...39M) 73 Machalski & Engels (1994MNRAS.266L..69M) 74 Morganti et al. (1992MNRAS.254..546M) 75 Owen et al. (1988AJ.....95....1O) 76 Sandage et al. (1976ApJ...205..688S) 77 Sargent (1973ApJ...182L..13S) 78 Smith & Spinrad (1980PASP...92..553S) 79 Spinrad (1982PASP...94..397S) 80 Spinrad & Djorgovski (1984ApJ...285L..49S) 81 Spinrad et al. (1985ApJ...299L...7S) 82 Stickel & Kuehr (1994, Cat. <J/A+AS/105/67>) 83 Strittmatter et al. (1974ApJ...190..509S) 84 Strom et al. (1990A&A...227...19S) 85 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 86 Vigotti et al. (1989AJ.....98..419V) 87 Walsh et al. (1979MNRAS.189..667W) 88 Warner et al. (1983MNRAS.204.1279W) 89 Wilkinson et al. (1981MNRAS.196..669W) 90 Zwicky & Herzog (1963, See Cat. <VII/4>) 91 LaHulla et al. (1991A&AS...88..525L) 92 Vermeulen et al. (1996AJ....111.1013V) 93 Sanghera et al. (1995A&A...295..629S) 94 Maxfield et al. (1995PASP..107..369M) References to X-ray data X1 Crawford & Fabian (1996MNRAS.282.1483C) X2 ROSAT Catalogue (See e.g. Cat. <IX/11>) X3 Worrall & Wilkes (1990ApJ...360..396W) X4 Wilkes et al. 1994, Cat. <J/ApJS/92/53> X5 Machalski & Brandt (1996MNRAS.282.1305M) --- Ref4 References to redshift number=9 References to VLA maps 1 Antonucci (1985ApJS...59..499A) 2 Burns et al. (1983ApJ...271..575B) 3 Capetti et al. (1993A&AS...99..407C) 4 Condon (1983ApJS...53..459C) 5 Condon & Broderick (1988AJ.....96...30C) 6 de Ruiter et al. (1986A&AS...65..111D) 7 Fanti et al. (1986A&AS...65..145F) 8 Fanti et al. (1987A&AS...69...57F) 9 Ford et al. (1985ApJ...293..132F) 10 Gioia & Fabbiano (1987ApJS...63..771G) 11 Hummel et al. (1985A&AS...60..293H) 12 Leahy & Perley (1991AJ....102..537L) 13 Lonsdale et al. (1993ApJS...87...63L) 14 Machalski et al. (1982AJ.....87.1150M), Paper II 15 Machalski & Condon (1983AJ.....88..143M), Paper III 16 Machalski & Condon (1983AJ.....88.1591M), Paper IV 17 Machalski & Condon (1985AJ.....90....5M), Paper V 18 Machalski & Condon (1985AJ.....90..973M) 19 Machalski & Condon (1986AJ.....91..998M) 20 Maslowski & Kellermann (1988AJ.....95.1659M) 21 O'Donoghue et al. (1993ApJ...408..428O) 22 Owen & Puschell (1984AJ.....89..932O) 23 Parma et al. (1986A&AS...64..135P) 24 Perley et al. (1980AJ.....85..649P) 25 Perley (1982AJ.....87..859P) 26 Perley et al. (1982ApJ...255L..93P) 27 Reid et al. (1995A&AS..110..213R) 28 Vallee et al. (1981ApJ...250...66V) 29 Vallee & Wilson (1976Natur.259..451V) 30 van Albada & van der Hulst (1982A&A...115..263V) 31 Vigotti et al. (1989A&AS...36..237W) 32 4885-MHz map in Figure A1. (Appendix) References to VLBI maps. 40 Henstock et al. (1995, Cat. <J/ApJS/100/1>) 41 Morabito et al. (1986AJ.....91.1038M) 42 Pearson & Readhead (1988ApJ...328..114P) 43 Polatidis et al. (1995, Cat. <J/ApJS/98/1>) 44 Thakkar et al. (1995, Cat. <J/ApJS/98/33>) 45 Xu et al. (1995, Cat. <J/ApJS/99/297>) 46 Rioja et al. (1996, Proc. IAU Symp. No.175, p.122) 47 Fey et al. (1996ApJS..105..299F) References to photometry 50 Allington-Smith et al. (1982MNRAS.201..331A) 51 Laing et al. (1983MNRAS.204..151L) 52 Machalski & Wisniewski (1988MNRAS.231.1065M) 53 Machalski (1992AcA....42..335M) 54 Machalski & Magdziarz (1993A&AS..102..315M) 57 Sandage (1972ApJ...176...21S) of Pointed Observations 55 Machalski & LaFranca (1988IAUC.4573.....M) 56 Moles et al. (1985A&A...152..271M) 58 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 59 Netzer et al. (1996MNRAS.279..429N) 591 Hook et al. (1996MNRAS.282.1274H) References to redshift 60 Allington-Smith et al. (1988MNRAS.234.1091A) 61 Burbidge (1970ApJ...160L..33B) 62 Burbidge & Strittmatter (1972ApJ...172L..37B) 63 Djorgovski et al. (1990PASP..102..113D) 64 Grueff et al. (1980A&A....86...50G) 65 Grueff & Vigotti (1979A&AS...35..371G) 66 Henstock (1995, priv. info.) 67 Hewitt & Burbidge (1993ApJS...87..451H, Cat. <VII/158>) 68 Huchra et al. (1983ApJS...52...89H, Cat. <VII/193>) 69 Katgert-Merkelijn et al. (1980A&AS...40...91K) 70 Laing et al. (1983MNRAS.204..151L) 71 Lilly et al. (1985MNRAS.215...37L) 72 Machalski (1991AcA....41...39M) 73 Machalski & Engels (1994MNRAS.266L..69M) 74 Morganti et al. (1992MNRAS.254..546M) 75 Owen et al. (1988AJ.....95....1O) 76 Sandage et al. (1976ApJ...205..688S) 77 Sargent (1973ApJ...182L..13S) 78 Smith & Spinrad (1980PASP...92..553S) 79 Spinrad (1982PASP...94..397S) 80 Spinrad & Djorgovski (1984ApJ...285L..49S) 81 Spinrad et al. (1985ApJ...299L...7S) 82 Stickel & Kuehr (1994, Cat. <J/A+AS/105/67>) 83 Strittmatter et al. (1974ApJ...190..509S) 84 Strom et al. (1990A&A...227...19S) 85 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 86 Vigotti et al. (1989AJ.....98..419V) 87 Walsh et al. (1979MNRAS.189..667W) 88 Warner et al. (1983MNRAS.204.1279W) 89 Wilkinson et al. (1981MNRAS.196..669W) 90 Zwicky & Herzog (1963, See Cat. <VII/4>) 91 LaHulla et al. (1991A&AS...88..525L) 92 Vermeulen et al. (1996AJ....111.1013V) 93 Sanghera et al. (1995A&A...295..629S) 94 Maxfield et al. (1995PASP..107..369M) References to X-ray data X1 Crawford & Fabian (1996MNRAS.282.1483C) X2 ROSAT Catalogue (See e.g. Cat. <IX/11>) X3 Worrall & Wilkes (1990ApJ...360..396W) X4 Wilkes et al. 1994, Cat. <J/ApJS/92/53> X5 Machalski & Brandt (1996MNRAS.282.1305M) --- Ref5 References to X-ray data number=9 References to VLA maps 1 Antonucci (1985ApJS...59..499A) 2 Burns et al. (1983ApJ...271..575B) 3 Capetti et al. (1993A&AS...99..407C) 4 Condon (1983ApJS...53..459C) 5 Condon & Broderick (1988AJ.....96...30C) 6 de Ruiter et al. (1986A&AS...65..111D) 7 Fanti et al. (1986A&AS...65..145F) 8 Fanti et al. (1987A&AS...69...57F) 9 Ford et al. (1985ApJ...293..132F) 10 Gioia & Fabbiano (1987ApJS...63..771G) 11 Hummel et al. (1985A&AS...60..293H) 12 Leahy & Perley (1991AJ....102..537L) 13 Lonsdale et al. (1993ApJS...87...63L) 14 Machalski et al. (1982AJ.....87.1150M), Paper II 15 Machalski & Condon (1983AJ.....88..143M), Paper III 16 Machalski & Condon (1983AJ.....88.1591M), Paper IV 17 Machalski & Condon (1985AJ.....90....5M), Paper V 18 Machalski & Condon (1985AJ.....90..973M) 19 Machalski & Condon (1986AJ.....91..998M) 20 Maslowski & Kellermann (1988AJ.....95.1659M) 21 O'Donoghue et al. (1993ApJ...408..428O) 22 Owen & Puschell (1984AJ.....89..932O) 23 Parma et al. (1986A&AS...64..135P) 24 Perley et al. (1980AJ.....85..649P) 25 Perley (1982AJ.....87..859P) 26 Perley et al. (1982ApJ...255L..93P) 27 Reid et al. (1995A&AS..110..213R) 28 Vallee et al. (1981ApJ...250...66V) 29 Vallee & Wilson (1976Natur.259..451V) 30 van Albada & van der Hulst (1982A&A...115..263V) 31 Vigotti et al. (1989A&AS...36..237W) 32 4885-MHz map in Figure A1. (Appendix) References to VLBI maps. 40 Henstock et al. (1995, Cat. <J/ApJS/100/1>) 41 Morabito et al. (1986AJ.....91.1038M) 42 Pearson & Readhead (1988ApJ...328..114P) 43 Polatidis et al. (1995, Cat. <J/ApJS/98/1>) 44 Thakkar et al. (1995, Cat. <J/ApJS/98/33>) 45 Xu et al. (1995, Cat. <J/ApJS/99/297>) 46 Rioja et al. (1996, Proc. IAU Symp. No.175, p.122) 47 Fey et al. (1996ApJS..105..299F) References to photometry 50 Allington-Smith et al. (1982MNRAS.201..331A) 51 Laing et al. (1983MNRAS.204..151L) 52 Machalski & Wisniewski (1988MNRAS.231.1065M) 53 Machalski (1992AcA....42..335M) 54 Machalski & Magdziarz (1993A&AS..102..315M) 57 Sandage (1972ApJ...176...21S) of Pointed Observations 55 Machalski & LaFranca (1988IAUC.4573.....M) 56 Moles et al. (1985A&A...152..271M) 58 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 59 Netzer et al. (1996MNRAS.279..429N) 591 Hook et al. (1996MNRAS.282.1274H) References to redshift 60 Allington-Smith et al. (1988MNRAS.234.1091A) 61 Burbidge (1970ApJ...160L..33B) 62 Burbidge & Strittmatter (1972ApJ...172L..37B) 63 Djorgovski et al. (1990PASP..102..113D) 64 Grueff et al. (1980A&A....86...50G) 65 Grueff & Vigotti (1979A&AS...35..371G) 66 Henstock (1995, priv. info.) 67 Hewitt & Burbidge (1993ApJS...87..451H, Cat. <VII/158>) 68 Huchra et al. (1983ApJS...52...89H, Cat. <VII/193>) 69 Katgert-Merkelijn et al. (1980A&AS...40...91K) 70 Laing et al. (1983MNRAS.204..151L) 71 Lilly et al. (1985MNRAS.215...37L) 72 Machalski (1991AcA....41...39M) 73 Machalski & Engels (1994MNRAS.266L..69M) 74 Morganti et al. (1992MNRAS.254..546M) 75 Owen et al. (1988AJ.....95....1O) 76 Sandage et al. (1976ApJ...205..688S) 77 Sargent (1973ApJ...182L..13S) 78 Smith & Spinrad (1980PASP...92..553S) 79 Spinrad (1982PASP...94..397S) 80 Spinrad & Djorgovski (1984ApJ...285L..49S) 81 Spinrad et al. (1985ApJ...299L...7S) 82 Stickel & Kuehr (1994, Cat. <J/A+AS/105/67>) 83 Strittmatter et al. (1974ApJ...190..509S) 84 Strom et al. (1990A&A...227...19S) 85 Veron-Cetty & Veron (1993, see Cat. <VII/188>) 86 Vigotti et al. (1989AJ.....98..419V) 87 Walsh et al. (1979MNRAS.189..667W) 88 Warner et al. (1983MNRAS.204.1279W) 89 Wilkinson et al. (1981MNRAS.196..669W) 90 Zwicky & Herzog (1963, See Cat. <VII/4>) 91 LaHulla et al. (1991A&AS...88..525L) 92 Vermeulen et al. (1996AJ....111.1013V) 93 Sanghera et al. (1995A&A...295..629S) 94 Maxfield et al. (1995PASP..107..369M) References to X-ray data X1 Crawford & Fabian (1996MNRAS.282.1483C) X2 ROSAT Catalogue (See e.g. Cat. <IX/11>) X3 Worrall & Wilkes (1990ApJ...360..396W) X4 Wilkes et al. 1994, Cat. <J/ApJS/92/53> X5 Machalski & Brandt (1996MNRAS.282.1305M) --- Note + : note detailed in file notes.dat --- Individual notes to table3.dat IAU IAU name --- Ntot Total number of lines for the reference --- Nline Running line number in range [1,Ntot] --- Com Comments --- table3a.tex LaTex version of the left part of table3.dat table3b.tex LaTex version of the right part of table3.dat notes.tex LaTeX version of the notes.dat file Patricia Bauer CDS 1997 Jul 03 Jerzy Machalski <machalsk@oa.uj.edu.pl> J_A+AS_128_153.xml Precision meteor orbits obtained by the Dutch Meteor Society - Photographic Meteor Survey (1981-1993) J/A+AS/128/179 J/A+AS/128/179 Precision meteor orbits Precision meteor orbits obtained by the Dutch Meteor Society - Photographic Meteor Survey (1981-1993) H Betlem C R ter Kuile M de Lignie J van't Leven K Jobse K Miskotte P Jenniskens Astron. Astrophys. Suppl. Ser. 128 179 1998 1998A&AS..128..179B Positional data Solar system Space velocities meteors, meteoroids Orbital elements, encounter data and other relevant information of 359 photographic meteors (Table 2 of the paper).
*Photographic orbital data of 359 multi station meteors Code DMS sequential numbering starting with the year --- Month Month --- Day Day and time (UT) in decimal days d Nstat Number of multi-station components --- Stream Meteor stream identification --- Mv Absolute visual magnitude at a distance of 100km mag q Perihelion distance AU e_q rms uncertainty on q AU a Semi-major axis AU 1/a Inverse semi-major axis AU-1 e_1/a rms uncertainty on AU-1 e Eccentricity --- e_e rms uncertainty on e --- i Inclination of the orbit with respect to the ecliptic (Eq. 2000) deg e_i rms uncertainty on i deg omega Argument of perihelion (Eq. 2000) deg e_omega rms uncertainty on omega deg Node Ascensing node (Eq. 2000) deg e_Node rms uncertainty on Node deg pi Longitude of perihelion (Eq. 2000) deg e_pi rms uncertainty on pi deg *Trajectory data of 359 multi station meteors Code DMS sequential numbering starting with the year --- Vg Geocentric velocity km/s Vh Heliocentric velocity km/s Vinf Apparent pre-atmospheric velocity km/s Vel Average velocity along trajectory km/s e_Vel rms uncertainty on Vel km/s Hbeg Beginning height km Hmax Height of brightest point on meteor track km Hend End height of meteor km RAdeg Apparent right ascension of radiant (2000) deg e_RAdeg Error due to uncertainty in time of meteor, or spread in solutions for all possible sets of two stations deg DEdeg Apparent declination of radiant (2000) deg e_DEdeg Error due to uncertainty in time of meteor, or spread in solutions for all possible sets of two stations deg RAgeo Geocentric right ascension of radiant (2000) deg DEgeo Geocentric declination (2000) deg CosZR Cosine of zenith angle of radiant at time of meteor --- Qmax Convergence angle between planes through meteor and photographic station, maximum value of all combinations deg Patricia Bauer CDS 1997 Jul 11 Hans Betlem <betlem@strw.leidenuniv.nl> J_A+AS_128_179.xml The Optical Gravitational lensing Experiment. Variable stars in globular clusters - IV. Fields 104A-E in 47 Tuc J/A+AS/128/19 J/A+AS/128/19 Variable stars in 47 Tuc fields 104A-E The Optical Gravitational lensing Experiment. Variable stars in globular clusters - IV. Fields 104A-E in 47 Tuc J Kaluzny M Kubiak M Szymanski A Udalski W Krzeminski M Mateo K Z Stanek Astron. Astrophys. Suppl. Ser. 128 19 1998 1998A&AS..128...19K I/244 : OGLE General Catalog of Stars. I. (Szymanski+ 1996) II/213 : OGLE Galactic Bulge periodic var. stars. (Udalski+ 1996) J/A+AS/112/407 : Variable Stars in the Sculptor dwarf galaxy (Kaluzny+, 1995) J/A+AS/120/139 : Variables in Omega Cen I. Fields 5139A-C (Kaluzny+ 1996) J/A+AS/122/471 : Variables in Omega Cen. II. Fields 5139D-F (Kaluzny+ 1997) J/A+AS/125/343 : Variables in Omega Cen. III. RR Lyr (Kaluzny+ 1997) Clusters, globular Photometry, CCD Stars, variable binaries: eclipsing blue stragglers globular clusters: individual (NGC 104) Hertzsprung-Russell (HR diagram) Magellanic Clouds stars: variables: other CCD photometry for 42 variables from the field of 47 Tuc = NGC 104 is presented. VI photometry for a large set of stars from the surveyed fields is also given.
NGC 104 47 Tuc 00 24 05.1 -72 04 51
V band light curve for variables OGLE 218, 239, 252 and 254 OGLE OGLE number --- HJD Heliocentric Julian date d Vmag V magnitude mag e_Vmag Internal error of V magnitude mag Phased V band light curve (tables 5 to 42) OGLE OGLE number --- HJD Heliocentric Julian date d Vmag V magnitude mag e_Vmag Internal error of V magnitude mag Phase Phase --- VI photometry for stars from 104A-E fields (tables 43 to 47) Field Field name (always 104) --- m_Field Multiplicity index in Field --- Xpos X coordinate number=1 The rectangular coordinates X & Y correspond to positions of stars on the "template" images (see paper for details). The X-axis points toward East an the Y axis points toward North. The scale is about 0.435 arcsec/pixel. pix Ypos Y coordinate number=1 The rectangular coordinates X & Y correspond to positions of stars on the "template" images (see paper for details). The X-axis points toward East an the Y axis points toward North. The scale is about 0.435 arcsec/pixel. pix RAdeg Right ascension in degrees, J2000 deg DEdeg Declination in degrees, J2000 deg Vmag V magnitude mag e_Vmag Internal error of V mag V-I V-I color mag e_V-I Internal error of V-I mag Patricia Bauer CDS 1997 Sep 09 Janusz Kaluzny (OGLE-1 team) <jka@vela.astrouw.edu.pl> J_A+AS_128_19.xml The electron impact broadening parameters in hot atmospheres: Mn II, Mn III, Ga III, Ge III and Ge IV lines J/A+AS/128/203 J/A+AS/128/203 Stark broadening of Mn, Ga & Ge multiplets The electron impact broadening parameters in hot atmospheres: Mn II, Mn III, Ga III, Ge III and Ge IV lines L C Popovic M S Dimitrijevic Astron. Astrophys. Suppl. Ser. 128 203 1998 1998A&AS..128..203P VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines J/A+AS/127/295 : Stark broadening of Kr II lines J/A+AS/127/543 : Stark broadening of S V lines J/A+AS/128/359 : Stark broadening of Ca IX and Ca X lines Atomic physics atomic data line: profiles stars: chemically peculiar The electron - impact line widths and shifts for 16 Mn II, 3 Mn III, 10 Ga III, 8 Ge III and 14 Ge IV multiplets, have been considered within a modified semiempirical approach. Moreover, using a semiclassical approach, we have considered electron-, proton-, and He III-impact line widths and shifts for 3 Ge IV multiplets. The obtained results have been compared with other theoretical results.
*Stark full widths (FWHM) of and shift for Mn II, Mn III, GA III and Ge III and Ge IV multiplets as a function of temperature. Ion Ion --- Tr Transition --- lambda Averaged wavelength of the multiplet 0.1nm T Temperature K W Stark width nm d Stark shift nm The electron-, proton-, and He III-impact broadening, full widths (FWHM) and shifts, for 3 Ge IV multiplets as a function of temperature and perturber density. N Perturber density m-3 Ion Ion --- Tr Transition --- lambda Averaged wavelength of the multiplet 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum nm n_de (4) --- de Shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid nm n_dp (4) --- dp Shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid nm n_WHe++ (4) --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum nm n_dHe++ (4) --- dHe++ Shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) nm tables.tex TeX version of tables 1, 2 and 3 Patricia Bauer CDS 1997 Sep 04 Dr. Luka C. Popovic <lpopovic@aob.bg.ac.yu> J_A+AS_128_203.xml uvby photometry of the chemically peculiar stars AR Aurigae, 3 Hydrae, 49 Cancri, and BX Boo J/A+AS/128/245 J/A+AS/128/245 Photometry of chemically peculiar stars uvby photometry of the chemically peculiar stars AR Aurigae, 3 Hydrae, 49 Cancri, and BX Boo S J Adelman Astron. Astrophys. Suppl. Ser. 128 245 1998 1998A&AS..128..245A J/A+AS/103/1 : 63 And, HD 192913, HR 8240 & 108 Aqr (Adelman+ 1994) J/A+AS/106/333 : Alpha And, HD 184905, HR 8216 & HR 8434 (Adelman+ 1994) J/A+AS/114/253 : HD 11187, HD 14940,HD 15144,20 Eri,HR 8933 (Adelman+ 1995) J/A+AS/122/249 : HD 32633, 25 Sex, HR 7224 & HD 200311 (Adelman, 1997) J/A+AS/125/65 : HD 37776, HR 2258, HR 6958 & 108 Aqr (Adelman, 1997) J/PASP/109/9 : HR 1643, Theta Aur, 49 Cam, and HR 3724 (Adelman 1997) Photometry, uvby Stars, peculiar stars: chemically peculiar stars: individual (AR Aur, 3 Hyd, 49 Can, BX Boo) Differential Stroemgren uvby photometric observations from the Four College Automated Photoelectric Telescope are presented for four Chemically Peculiar stars of the upper main sequence: the HgMn star binary AR Aurigae and the magnetic stars 3 Hydrae, 49 Cancri, and BX Bootis. AR Aurigae shows little variability except during the primary and secondary eclipses. The 11.305 day period of Maitzen et al. for 3 Hya is confirmed. A new period of 7.0501 days is found for 49 Cancri while a slightly refined period of 2.88756 days is derived for BX Boo.
AR Aur HD 34364 HR 1728 05 18 18.8 +33 46 03 HD 72968 3 Hya HR 3398 08 35 28.2 -07 58 57 HD 74521 49 Cnc HR 3465 08 44 45.0 +10 04 55 BX Boo HD 133029 HR 5597 15 00 38.7 +47 16 38
Photometry of AR Aur Photometry of 3 Hya Photometry of 49 Cnc Photometry of BX Boo HJD Heliocentric Julian Date d u(v-c) variable-comparison (v-c) u magnitude mag u(ch-c) check-comparison (ch-c) u magnitude mag b(v-c) variable-comparison (v-c) b magnitude mag b(ch-c) check-comparison (ch-c) b magnitude mag v(v-c) variable-comparison (v-c) v magnitude mag v(ch-c) check-comparison (ch-c) v magnitude mag y(v-c) variable-comparison (v-c) y magnitude mag y(ch-c) check-comparison (ch-c) y magnitude mag Average values Name Star name --- Per Period considered (in the form 1990-91) --- Note Note on period --- u(v-c) variable-comparison (v-c) u magnitude mag e_u(v-c) rms uncertainty on u(v-c) mag u(ch-c) check-comparison (ch-c) u magnitude mag e_u(ch-c) rms uncertainty on u(ch-c) mag v(v-c) variable-comparison (v-c) v magnitude mag e_v(v-c) rms uncertainty on v(v-c) mag v(ch-c) check-comparison (ch-c) v magnitude mag e_v(ch-c) rms uncertainty on v(ch-c) mag b(v-c) variable-comparison (v-c) b magnitude mag e_b(v-c) rms uncertainty on b(v-c) mag b(ch-c) check-comparison (ch-c) b magnitude mag e_b(ch-c) rms uncertainty on b(ch-c) mag y(v-c) variable-comparison (v-c) y magnitude mag e_y(v-c) rms uncertainty on y(v-c) mag y(ch-c) check-comparison (ch-c) y magnitude mag e_y(ch-c) rms uncertainty on y(ch-c) mag Patricia Bauer CDS 1997 Sep 04 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> UNKNOWN UNKNOWN There were an inversion between the b and v magnitude labels. This was corrected on 24-Apr-1998 J_A+AS_128_245.xml Four-colour photometry of eclipsing binaries. XXXVI. Light curves of the O7V+O9V system V3903 Sagittarii J/A+AS/128/251 J/A+AS/128/251 uvby photometry of V3903 Sgr Four-colour photometry of eclipsing binaries. XXXVI. Light curves of the O7V+O9V system V3903 Sagittarii L P R Vaz N C S Cunha J Andersen J V Clausen J M Garcia A Gimenez B W Casey S de Koff Astron. Astrophys. Suppl. Ser. 128 251 1998 1998A&AS..128..251V Binaries, eclipsing Photometry, uvby binaries: eclipsing binaries: spectroscopic stars: early-type stars: individual (V3903 Sgr) Complete uvby light curves of the young detached double-lined massive O-type eclipsing binary V3903 Sagittarii, obtained from 1989 to 1994, are presented. The observations were obtained at two different sites and a discussion of the characteristics of both data sets is included.
V3903 Sgr HD 165921 18 09 17.7 -23 59 18 HD 165999 18 09 36.1 -23 34 04
*uvby magnitude differences V3903 Sgr - HD 165999 obtained at PDO from 1989 to 1991 HJDu Heliocentric Julian Day u colour d umag Magnitude u mag HJDv Heliocentric Julian Day v colour d vmag Magnitude v mag HJDb Heliocentric Julian Day b colour d bmag Magnitude b mag HJDy Heliocentric Julian Day y colour) d ymag Magnitude y mag magnitude differences V3903 Sgr - HD 165999 obtained at ESO from 1990 to 1993 (instrumental system) magnitude differences V3903 Sgr - HD 165999 obtained at ESO in 1994 (instrumental system) HJD Heliocentric Julian Day d ymag Magnitude y mag b-y Colour index b-y mag m1 Stroemgren index m1 mag c1 Stroemgren index c1 mag bmag Magnitude b mag vmag Magnitude v mag umag Magnitude u mag Patricia Bauer CDS 1997 Jul 22 Luiz Paulo R. Vaz <vaz@suya.fisica.ufmg.br> J_A+AS_128_251.xml Membership determination of stars using proper motions in the region of the open cluster M11 J/A+AS/128/255 J/A+AS/128/255 Proper motions in M 11 Membership determination of stars using proper motions in the region of the open cluster M11 C -G Su J -L Zhao K -P Tian Astron. Astrophys. Suppl. Ser. 128 255 1998 1998A&AS..128..255S Clusters, open Proper motions membership determination open clusters and associations: general open clusters and associations: individual (M 11) proper motions Relative proper motions of 872 stars in the open cluster M 11 region are reduced using 10 plate pairs taken over time baselines of 16~70 years with the double astrograph telescope of Shanghai Observatory. The scale is 30"/mm. The plates were measured with the PDS machines in the Purple Mountain Observatory in Nanjing and the Institute of Technology and Communication in Luoyang, China. The average proper motion accuracy is about 1.1mas/yr with 85% of the data better than 1mas/yr. Membership probabilities of 785 stars within 25' centred on M 11 are determined based on their proper motions. The method used is suggested by Su et al. (1995AcApS..15..202S) with some improvements of Zhao & He (1990A&A...237...54Z), in which the space distribution and magnitude dependencies for cluster stars are taken into account. The results are significantly good. The total integrated membership probabilities for all these stars is 547 and the number of stars with probabilities higher than 0.7 is 541. It can be found after the membership determination that there exists mass segregation in M 11. Some comparisons and discussion are also given.
M 11 NGC 6705 18 51.1 -06 16
Relative proper motions and membership probabilities of stars in the M11 region Star Star number --- n_Star *: Reference star --- NSP Star number in the catalogue of McNamara, Sanders & Pratt (1977A&AS...27..117M) --- Xpos Measured coordinate in X number=1 1 mm = 30" cm Ypos Measured coordinate in Y number=1 1 mm = 30" cm Vmag V magnitude mag Bmag B magnitude mag pmX Relative proper motion in X 10-2arcsec/yr pmY Relative proper motion in Y 10-2arcsec/yr e_pmX Uncertainty of proper motion in X 10-2arcsec/yr e_pmY Uncertainly of proper motion in Y 10-2arcsec/yr Nplate Number of the plate pairs --- Member Membership probability % Francois Ochsenbein CDS 1997 Jul 15 Tian Kaiping <tkp@center.shao.ac.cn> J_A+AS_128_255.xml CP2 stars as viewed by the ubvy-beta system J/A+AS/128/265 J/A+AS/128/265 ubvy-beta photometry of CP2 stars CP2 stars as viewed by the ubvy-beta system E Masana C Jordi H M Maitzen J Torra Astron. Astrophys. Suppl. Ser. 128 265 1998 1998A&AS..128..265M III/162 : General Catalogue of Ap and Am stars (Renson+ 1991) Photometry, uvby, beta Stars, early-type Stars, peculiar stars: chemically peculiar stars: early-type stars: fundamental parameters The aim of this work is to study the capacity of the uvby H_{beta}_ system for detecting the chemically peculiar (CP) stars based on the effect that peculiar features in the flux distribution have on all the Stroemgren-Crawford indices. Our study focuses on the classical magnetic peculiar stars (CP2), though Am star s (CP1) are also included for comparison with cool CP2 stars. Satisfactory results were obtained for hot CP2 stars: the definition of a new index p, which is a linear combination of uvby H_{beta}_ colours, allowed us to separate a high percentage of hot CP2 stars from normal stars. According to this new index, 60 new CP2 candidates are proposed. The working sample was extracted from The General Catalogue of Ap and Am stars by Renson et al. (1991, Cat. <III/162>). Photometric observations to enlarge the sample of CP2 stars with complete uvby H_{beta}_ photometry were carried out. These observations are also reported in the present paper. The new index p is also used to correct the reddening of early CP2 stars computed as if they were normal stars.
uvby-beta photometry for CP2 stars HD Identification (HD number, Cat. <III/135>) --- m_HD Multiplicity index on HD --- HIC Identification (HIC number, Cat. <I/196>) --- m_HIC Multiplicity index on HIC --- SpType Spectral type --- (b-y) (b-y) colour index mag e_(b-y) rms uncertainty (b-y) mag Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag m1 m1 colour index mag e_m1 rms uncertainty on m1 mag c1 c1 colour index mag e_c1 rms uncertainty on c1 mag o_uvby Number of measurements in uvby --- Hbeta H{beta} colour index mag e_Hbeta rms uncertainty Hbeta mag o_Hbeta Number of measurements in H{beta} --- H{beta} photometry for CP2 stars HD Identification (HD number, Cat. <III/135>) --- m_HD Multiplicity index on HD --- HIC Identification (HIC number, Cat. <I/196>) --- m_HIC Multiplicity index on HIC --- SpType Spectral type --- Hbeta H{beta} colour index mag e_Hbeta rms uncertainty on Hbeta mag o_Hbeta Number of measurements in H{beta} --- Early CP2 candidate stars Name Identification number=1 references of the numeration for the cluster star in Table 7. Mel 20: Heckmann O., et al., 1956MiHam..10...37H 1956, Mitt. Hamburg. Sternw. Bergedorf, no. 10 NGC 1893: Cuffey J., 1937AnHar.105..403C NGC 2244: Ogura K., Ishida K., 1981PASJ...33..149O NGC 2516: Cox A.N., 1955ApJ...121..628C NGC 3293: Turner D.G., et al., 1980AJ.....85.1193T NGC 3766: Ahmed F., 1962PROE....3...57A NGC 6231: Seggewis W., 1968VeBon..79....1S NGC 7039: Hassan S.M., 1973A&AS....9..261H NGC 7243: Lengauer G.G., 1937, Izv. Glav. Astr. Obs. Pulkove 15, no. 126 =1937BOPul..15....3L NGC 7654: Lundby A., 1946UppAn...1j...1L IC 4725: Johnson H.L., 1960ApJ...131..620J --- OtherName Alternative identification number=1 references of the numeration for the cluster star in Table 7. Mel 20: Heckmann O., et al., 1956MiHam..10...37H 1956, Mitt. Hamburg. Sternw. Bergedorf, no. 10 NGC 1893: Cuffey J., 1937AnHar.105..403C NGC 2244: Ogura K., Ishida K., 1981PASJ...33..149O NGC 2516: Cox A.N., 1955ApJ...121..628C NGC 3293: Turner D.G., et al., 1980AJ.....85.1193T NGC 3766: Ahmed F., 1962PROE....3...57A NGC 6231: Seggewis W., 1968VeBon..79....1S NGC 7039: Hassan S.M., 1973A&AS....9..261H NGC 7243: Lengauer G.G., 1937, Izv. Glav. Astr. Obs. Pulkove 15, no. 126 =1937BOPul..15....3L NGC 7654: Lundby A., 1946UppAn...1j...1L IC 4725: Johnson H.L., 1960ApJ...131..620J --- SpType Spectral type --- DELTAp Delta p (peculiarity parameter) mag Patricia Bauer CDS 1997 Jul 24 Eduard Masana <emasana@fajtr0.am.ub.es> J_A+AS_128_265.xml X-ray/optical observations of stars with shallow convection zones (A8-G2 V) J/A+AS/128/29 J/A+AS/128/29 X-ray/optical observations of A8-G2V stars X-ray/optical observations of stars with shallow convection zones (A8-G2 V) A J M Piters J Van Paradijs J H M M Schmitt Astron. Astrophys. Suppl. Ser. 128 29 1998 1998A&AS..128...29P Effective temperatures Photometry, VBLUW Stars, dwarfs X-ray sources stars: activity stars: fundamental parameters X-rays: stars Table 1 lists the sample of 173 stars observed for this study. They are selected from the Bright Star Catalogue (Cat. <V/50>), with the following selection criteria: - Spectral type between A8 and G2; no spectral peculiarities noted; not double in spectral type classification (e.g., HR 32 with spectral type F2V+F6V is excluded); - Luminosity class V; - Right ascension between 0h and 2h, or between 14h and 24 h, declination south of +10 degrees (defining the region on the sky visible during the appointed observation times); - Binaries for which both components occurred in the BSC are excluded, if the separation is less than 10". Not listed are five stars for which no (Walraven photometric and ROSAT X-ray) data are available. These are HR 591, HR 5542, HR 6593, HR 8245 and HR 8735. Table 2 lists the Walraven photometric (VBLUW) data for all but four stars from Table 1. Also listed in Table 2 are the effective temperature, surface gravity and the reddening, as derived from comparison with theoretical colours. Table 5 lists the ROSAT All Sky Survey data for all but 11 stars from Table 1. For a description of the Walraven photometric system, see e.g. <GCPD/11>
Sample stars HR HR (Cat. <V/50>) number --- Note See Note number=1 A: No Walraven data available B: No ROSAT data available --- Type Spectral Type number=2 Data from HR (Cat. <V/50>) catalog --- Vmag Apparent visual Johnson V magnitude number=2 Data from HR (Cat. <V/50>) catalog mag B-V Johnson's B-V colour number=2 Data from HR (Cat. <V/50>) catalog mag Walraven photometry data HR HR number (as in table1) --- Note See Note number=1 *: Probably variable: standard deviation of the brightness or one of the Walraven colours is more than 4 times as large as the average standard deviation. --- VWmag visual (Walraven) magnitude V mag e_VWmag standard deviation in VWmag mag V-B Walraven colour V-B mag e_V-B Standard deviation in V-B mag B-U Walraven colour B-U mag e_B-U Standard deviation in B-U mag U-W Walraven colour U-W mag e_U-W Standard deviation in U-W mag B-L Walraven colour B-L mag e_B-L Standard deviation in B-L mag o_B-L Number of observations --- Teff Effective temperature K e_Teff Uncertainty in Teff number=2 If the uncertainties are not given, no consistent stellar parameters could be found by the method applied here (minimum chi-square larger than 10). K logg Logarithm of surface gravity cm/s2 e_logg Uncertainty in logg number=2 If the uncertainties are not given, no consistent stellar parameters could be found by the method applied here (minimum chi-square larger than 10). cm/s2 E(V-B) The reddening E(V-B) mag e_E(V-B) Uncertainty in E_V-B number=2 If the uncertainties are not given, no consistent stellar parameters could be found by the method applied here (minimum chi-square larger than 10). mag ROSAT X-ray data HR HR number (as in table1) --- Note See Note number=1 U: upper limit values for Count, logRx, logFx, and logLx; hardness ratio h and the uncertainties (E_h, e_h, E_logRx, e_logRx, E_logFx, e_logFx, E_logLx, and e_logLx-) are not given (left blank). --- Count X-ray count rate s-1 E_Count Positive uncertainty in Count s-1 e_Count Negative uncertainty in Count s-1 XHR Hardness ratio --- E_XHR Positive uncertainty in XHR --- e_XHR Negative uncertainty in XHR --- logCx Log of energy-conversion factor number=2 The unit of the energy-conversion factor C_X_ is: cm^2/ergs, so that f_X_ = r_s_ / C_X_ is the flux density in ergs/(sec.cm^2) received at the detector. [10+7cm2/J] E_logCx Positive uncertainty in logCx [10+7cm2/J] e_logCx Negative uncertainty in logCx [10+7cm2/J] lognH Logarithm of hydrogen column density [cm-2] e_lognH Uncertainty in lognH [cm-2] logRx Log of Normalized X-ray flux density number=3 log Rx = log f_X_ + 0.1(V_J_ + BC) + 4.574 (BC: bolometric correction) log Fx = log Rx + 4logTeff - 4.246 log Lx = log Fx + 2log(R*/R_{sun}_) + 22.784 --- E_logRx Positive uncertainty in logRx --- e_logRx Negative uncertainty in logRx --- logFx Log of X-ray surface flux density number=3 log Rx = log f_X_ + 0.1(V_J_ + BC) + 4.574 (BC: bolometric correction) log Fx = log Rx + 4logTeff - 4.246 log Lx = log Fx + 2log(R*/R_{sun}_) + 22.784 --- E_logFx Positive uncertainty in logFx --- e_logFx Negative uncertainty in logFx --- logLx Logarithmic X-ray luminosity number=3 log Rx = log f_X_ + 0.1(V_J_ + BC) + 4.574 (BC: bolometric correction) log Fx = log Rx + 4logTeff - 4.246 log Lx = log Fx + 2log(R*/R_{sun}_) + 22.784 --- E_logLx Positive uncertainty in logLx --- e_logLx Negative uncertainty in logLx --- Ankie Piters Astron. Inst., Amsterdam Patricia Bauer CDS 1997 Sep 09 Ankie Piters <piters@knmi.nl> J_A+AS_128_29.xml Stroemgren and H{beta} photometry of OB stars in the region of the Carina Spiral Feature J/A+AS/128/309 J/A+AS/128/309 ubvy-beta photometry of CarOB1 and CarOB2 stars Stroemgren and H{beta} photometry of OB stars in the region of the Carina Spiral Feature N T Kaltcheva Astron. Astrophys. Suppl. Ser. 128 309 1998 1998A&AS..128..309K Associations, stellarPhotometry, uvby, beta Stars, OB Galaxy: structure Hertzsprung-Russell (HR diagram) stars: distances stars: early-type Stromgren and H{beta} photometry of 130 stars in the Carina section of the Milky Way is presented. The color excesses and the distances of all stars are obtained. A good agreement is found between the CM and HR diagrams and the spatial distribution of these stars.
Stromgren and H{beta} data for 50 stars in Carina OB1 field. Stromgren and H{beta} data for 80 stars in Carina OB2 field. HD HD (Cat. <III/135>) number --- m_HD Multiplicity index on HD --- Vmag V magnitude mag b-y b-y colour index mag m1 m1 colour index mag c1 c1 colour index mag beta H{beta} colour index mag Car OB1 - derived quantities Car OB2 field - derived quantities HD HD number --- m_HD Multiplicity index on HD --- SpType MK type, remark --- (b-y)0 Derredened b-y colour mag m0 Derredened m0 colour index mag c0 Derredened c0 colour index mag E(b-y) Interstellar extinction mag V0 Derredened V magnitude mag Mv Absolute V magnitude mag u_Mv Uncertainty flag on Mv --- V0-Mv Distance modulus mag u_V0-Mv Uncertainty flag on V0-Mv --- r Distance pc u_r Uncertainty flag on r --- Other stars with Stromgren and H{beta} photometry in the same fields. HD Hd number --- Field Field (CarOB1 or Car OB2) --- SpType MK type --- Ref Reference number=1 K&W: Kilkenny D. & Whittet D., 1985MNRAS.216..127K Z: Zhang E.-Ho., 1983AJ.....88..825Z G&O: Gray & Olsen E., 1991A&AS...87..541G K: Knude J. 1992, Cat. <J/A+AS/92/841> --- (b-y)0 Deredenned b-y colour mag m0 Deredenned m1 colour mag c0 Deredenned c1 colour mag E(b-y) Interstellar extinction mag V0 Deredenned V magnitude mag Mv Absolute V magnitude mag V0-Mv Distance modulus mag r Distance pc Stars with UBV H{beta} photometry in the same fields HD HD name --- Field Fields (CarOB1 or CarOB2) --- Vmag V magnitude mag beta H{beta} colour index mag SpType MK spectral classification --- B-V B-V colour index mag Mv Absolute V magnitude mag u_Mv Uncertainty flag on Mv --- E(b-y) Interstellar extinction mag V0-Mv Distance modulus mag r Distance pc Patricia Bauer CDS 1997 Oct 21 Nadia Kaltcheva <matey@csd.uwm.edu> J_A+AS_128_309.xml Searching for Old Neutron Stars with ROSAT: I. Soft X-ray Sources in Molecular Clouds at High Galactic Latitude. J/A+AS/128/331 J/A+AS/128/331 X-ray Sources in Molecular Clouds Searching for Old Neutron Stars with ROSAT: I. Soft X-ray Sources in Molecular Clouds at High Galactic Latitude. R Danner Astron. Astrophys. Suppl. Ser. 128 331 1998 1998A&AS..128..331D J/A+A/316/147 : Catalogue of ROSAT White Dwarfs (Fleming+ 1996) Danner, Paper II. 1998A&AS..128..349D X-ray sources radio continuum: stars stars: neutron surveys white dwarfs X-rays: stars Figure 9: Finding charts for the objects where spectra were taken, based on the APM data base. The cross is centered at the X-ray position. 30 arcsec radius error circles are shown and arrows mark the objects with the available spectra. North is up and East to the left in all charts. Figure 10: Deep CCD images of the X-ray source fields with faint optical counterparts. Circles with 30 arcsec radius are centered on the X-ray position. Capital letters identify the brightest object next to them (see Table 3 for remarks on identification). The filter used and the exposure time are shown above each image in brackets.
ROSAT
Summary of the identification program of all 89 sources found within the lowest contours of the MBM cloud maps ID Internal reference number --- RAh X-ray right ascension (2000.0) h RAm X-ray right ascension (2000.0) min RAs X-ray right ascension (2000.0) s DE- Declination sign --- DEd X-ray declination (2000.0) deg DEm X-ray declination (2000.0) arcmin DEs X-ray declination (2000.0) arcsec Rate Source count rate ct/s e_Rate Error in count rate ct/s HR1 Hardness ratio HR1 number=1 When blank, source was not detected when data were split into two spectral channels --- HR2 Hardness ratio HR2 number=1 When blank, source was not detected when data were split into two spectral channels --- Name Catalog name of object --- n_Name Note on Name number=2 *: new Identification +: new classification a: not detected in snapshot b: in visual binary with M4V --- SpType Spectral Type --- BandP Band of the magnitude mvis --- mvis Visual magnitude of counterpart mag l_O-E Limit flag on O-E --- O-E O-E color index from APM scans mag Dist Separation between X-ray source and proposed counterpart arcsec Band Bands in which the source has been observed at the VLA --- l_log(FX/Fopt) Limit flag on log(FX/Fopt) --- log(FX/Fopt) Logarithm of X-ray to optical flux ratio --- table2.tex LaTeX version of table2 fig9a.ps Finding charts fig9b.ps Finding charts fig9c.ps Finding charts fig9d.ps Finding charts fig9e.ps Finding charts fig9f.ps Finding charts fig10a.ps Deep CCD images fig10b.ps Deep CCD images fig10c.ps Deep CCD images fig10d.ps Deep CCD images fig10e.ps Deep CCD images fig10f.ps Deep CCD images Patricia Bauer CDS 1997 Aug 20 Rudolf Danner <rmd@astro.caltech.edu> J_A+AS_128_331.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest. XVII: Ca IX and Ca X spectral lines J/A+AS/128/359 J/A+AS/128/359 Stark broadening of Ca IX and Ca X lines Stark broadening of spectral lines of multicharged ions of astrophysical interest. XVII: Ca IX and Ca X spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 128 359 1998 1998A&AS..128..359D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines J/A+AS/127/295 : Stark broadening of Kr II lines J/A+AS/127/543 : Stark broadening of S V lines J/A+AS/128/203 : Stark broadening of Mn, Ga & Ge multiplets Atomic physics atomic data line: profiles plasmas Using a semiclassical approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 Ca IX multiplets for perturber densities 10^18^-10^22^cm^-3^ and 48 Ca X multiplets for perturber densities 10^17^-10^22^cm^-3^. In both cases the temperature range is T=200000-5000000K. For lower perturber densities, obtained results are linear with perturber density.
Stark broadening parameters due to e-, p- and He III-impacts for Ca IX and Ca X N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ (4) --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ (4) --- dHe++ shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1997 Jul 18 Dr Milan Dimitrijevic <mdimitrijevic@aob.aob.bg.ac.yu> J_A+AS_128_359.xml Table of vacuum ultraviolet emission band systems of molecular nitrogen from 82.6 to 124.2 nm J/A+AS/128/361 J/A+AS/128/361 Vacuum ultraviolet emission band systems of N2 Table of vacuum ultraviolet emission band systems of molecular nitrogen from 82.6 to 124.2 nm J -Y Roncin F Launay Astron. Astrophys. Suppl. Ser. 128 361 1998 1998A&AS..128..361R Atomic physics Spectra, ultraviolet molecular data planets and satellites: general The first column gives the rotational quantum number J of the electronic ground state. The corresponding R and P branch lines of the {SIGMA}-{SIGMA} transitions are listed in the second and third columns and the R, Q, and P branch lines of the {PI}-{SIGMA} transitions are listed in the second, third, and fourth columns. An asterisk is used to identify blended lines that have been assigned more than once, or to indicate, in the case of a missing line, that a feature has been observed within 1.2 and 2 cm-1 from the missing transition. For many missing lines we have written, in the same column, the name of the molecular absorption lines preventing the emission from being seen. Some missing lines could not be measured because they are overlapped by a strong atomic line which is identified in this column. Observed wavenumbers of the emission lines belonging to 10 vacuum ultraviolet band systems of molecular nitrogen are classified into 283 bands, 220 of them reported for the first time
Wavenumbers of R and P lines of the N2 band Band Band number=1 b'(i-j): b' ^1^{SIGMA}_u_+ -X ^1^{SIGMA}_g_+ band system of N2 c'4(i-j): c'4 ^1^{SIGMA}_u_+ -X ^1^{SIGMA}_g_+ band system of N2 c'6(i-j): c'6 ^1^{SIGMA}_u_+ -X ^1^{SIGMA}_g_+ band system of N2 3dp(0-1): 3dp ^1^{SIGMA}_u_+ -X ^1^{SIGMA}_g_+ band system of N2 --- J Rotational quantum number of the electronic ground state ---- R R branch lines of the {SIGMA}-{SIGMA} transitions number=2 Some missing lines could not be measured because they are overlapped by a strong atomic line which is identified in this column. cm-1 BlendR Blended line number=3 An asterisk is used to identify blended lines that have been assigned more than once, or to indicate, in the case of a missing line, that a feature has been observed within 1.2 and 2cm-1 from the missing transition --- n_R Note for missing line number=4 Name of the molecular absorption lines preventing the emission from being seen --- P P branch lines of the {SIGMA}-{SIGMA} transitions number=2 Some missing lines could not be measured because they are overlapped by a strong atomic line which is identified in this column. cm-1 BlendP Blended line number=3 An asterisk is used to identify blended lines that have been assigned more than once, or to indicate, in the case of a missing line, that a feature has been observed within 1.2 and 2cm-1 from the missing transition --- n_P Note for missing line number=4 Name of the molecular absorption lines preventing the emission from being seen --- Wavenumbers of R, Q and P lines of the N2 band Band Band number=1 b(i-j): b ^1^{PI}_u_ -X ^1^{SIGMA}_g_+ band system of N2 c3(i-j): c3 ^1^{PI}_u_ -X ^1^{SIGMA}_g_+ band system of N2 c4(0-j): c4 ^1^{PI}_u_ -X ^1^{SIGMA}_g_+ band system of N2 o3(i-j): o3 ^1^{PI}_u_ -X ^1^{SIGMA}_g_+ band system of N2 a(i-j): a ^1^{PI}_g_ -X ^1^{SIGMA}_g_+ band system (L.B.H.) of N2 --- J Rotational quantum number of the electronic ground state ---- R R branch lines of the {PI}-{SIGMA} transitions number=2 Some missing lines could not be measured because they are overlapped by a strong atomic line which is identified in this column. cm-1 BlendR Blended line number=3 An asterisk is used to identify blended lines that have been assigned more than once, or to indicate, in the case of a missing line, that a feature has been observed within 1.2 and 2cm-1 from the missing transition --- n_R Note for missing line number=4 Name of the molecular absorption lines preventing the emission from being seen --- Q Q branch lines of the {PI}-{SIGMA} transitions number=2 Some missing lines could not be measured because they are overlapped by a strong atomic line which is identified in this column. cm-1 BlendQ Blended line number=3 An asterisk is used to identify blended lines that have been assigned more than once, or to indicate, in the case of a missing line, that a feature has been observed within 1.2 and 2cm-1 from the missing transition --- n_Q Note for missing line number=4 Name of the molecular absorption lines preventing the emission from being seen --- P P branch lines of the {PI}-{SIGMA} transitions number=2 Some missing lines could not be measured because they are overlapped by a strong atomic line which is identified in this column. cm-1 BlendP Blended line number=3 An asterisk is used to identify blended lines that have been assigned more than once, or to indicate, in the case of a missing line, that a feature has been observed within 1.2 and 2cm-1 from the missing transition --- n_P Note for missing line number=4 Name of the molecular absorption lines preventing the emission from being seen --- Patricia Bauer CDS 1997 Nov 10 Jean-Yves Roncin <roncin@univ-st-etienne.fr> J_A+AS_128_361.xml Wavelength calibration at moderately high resolution J/A+AS/128/409 J/A+AS/128/409 Wavelength calibration Wavelength calibration at moderately high resolution J -P De Cuyper H Hensberge Astron. Astrophys. Suppl. Ser. 128 409 1998 1998A&AS..128..409D Spectroscopy methods: data analysis techniques: spectroscopic Thorium-Argon lamps are commonly used as wavelength calibration units at moderately high spectral resolutions because of the richness of the thorium spectrum in the visual. The inclusion of blended lines whose position is assumed to coincide with the laboratory wavelength of the main component is shown to result in a calibration precision significantly worse than the intrinsic random noise limit. In order to avoid this degradation of the calibration, we present resolution-dependent Th-Ar wavelengths in the region 277 to >1000nm for use at pixel-scales (pixel-size expressed in wavelength units) between {lambda}/2.5x10+4 and {lambda}/10+5.
*Principle table for the standard case of the argon-to-thorium line strength ratio *Principle table for the argon rich case Maincomp Laboratory wavelength of the main component 0.1nm Ion Ion emitting the main component --- Logint Relative log intensity of the main component --- lam025000 Blend wavelength for R=25000 0.1nm lam033333 Blend wavelength for R=33333 0.1nm lam043700 Blend wavelength for R=43700 0.1nm lam050000 Blend wavelength for R=50000 0.1nm lam100000 Blend wavelength for R=100000 0.1nm dp025 Displacement of the line for R=25000 pix s025 Discretisation stability of dp025 number=1 The parameter s is the r.m.s. of the blend wavelengths calculated for 20 different discretisations (sub-pixel locations of the line center) in steps of 0.05pix pix dp033 Displacement of the line for R=33333 pix s033 Discretisation stability of dp033 number=1 The parameter s is the r.m.s. of the blend wavelengths calculated for 20 different discretisations (sub-pixel locations of the line center) in steps of 0.05pix pix dp043 Displacement of the line for R=43700 pix s043 Discretisation stability of dp043 number=1 The parameter s is the r.m.s. of the blend wavelengths calculated for 20 different discretisations (sub-pixel locations of the line center) in steps of 0.05pix pix dp050 Displacement of the line for R=50000 pix s050 Discretisation stability of dp050 number=1 The parameter s is the r.m.s. of the blend wavelengths calculated for 20 different discretisations (sub-pixel locations of the line center) in steps of 0.05pix pix dp100 Displacement of the line for R=100000 pix s100 Discretisation stability of dp100 number=1 The parameter s is the r.m.s. of the blend wavelengths calculated for 20 different discretisations (sub-pixel locations of the line center) in steps of 0.05pix pix Selected lines R Lambda/pixel-scale number=1 Where lambda is the wavelength, and pixel-scale is the pixel-size expressed in wavelength units R = 25000; 33333; 43700; 50000; 100000 --- Lambda Pixel-scale dependent blend wavelength 0.1nm Maincomp Laboratory wavelength of the main component 0.1nm Ion Ion emitting the main component --- Jean-Pierre De Cuyper KSB/ORB 1997 May 15 Jean-Pierre De Cuyper <system@midasc.oma.be> Both authors carried out the research in the framework of projects initiated and financed by the Belgian Federal Scientific Services (DWTC/SSTC), under contract "Service Centres and Research Networks" nr. SC/005 and contract I.U.A.P. nr. P4/05. J_A+AS_128_409.xml New proper motion determination of Luyten catalogue stars (LTT) with declination between -5{deg} and -30{deg} and right ascension between 0h and 13h 30m. J/A+AS/128/457 J/A+AS/128/457 Proper motion LTT stars -5<DE<-30, 0<RA<13h30 New proper motion determination of Luyten catalogue stars (LTT) with declination between -5{deg} and -30{deg} and right ascension between 0h and 13h 30m. H Wroblewski C Torres Astron. Astrophys. Suppl. Ser. 128 457 1998 1998A&AS..128..457W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/83/317 : Proper-motion LTT stars Dec<-40, 0<RA<4h30 (Wroblewski+ 1990) J/A+AS/92/449 : Proper-motion LTT stars Dec<-40, 4h30<RA<16 (Wroblewski+ 1992) J/A+AS/110/27 : Proper motion LTT stars Dec<-40, 16<RA<24 (Wroblewski+, 1995) -------------------------------------------------------------------------------- Proper motions astrometry stars: kinematics Data are given for 353 LTT stars found on 42 areas, covering 25 square degrees each, with declination between -5{deg} and -30{deg} and right ascension between 0h and 13h 30m. Nineteen stars present differences in proper motion >=0.10", twenty present differences in position angle >=20{deg} and six present those differences in both values.
Proper motions and position angles ID Correlative number --- LTT Star number in Luyten's catalogue --- Loc Location number number=1 The first two digits refer to the area number and the other digits refer to the star number in the area --- mag Magnitude mag RA1950h Right ascension (1950) h RA1950m Right ascension (1950) min RA1950s Right ascension (1950) s DE1950- Declination sign --- DE1950d Declination (1950) deg DE1950m Declination (1950) arcmin DE1950s Declination (1950) arcsec RA2000h Right ascension (2000) h RA2000m Right ascension (2000) min RA2000s Right ascension (2000) s DE2000- Declination sign --- DE2000d Declination (2000) deg DE2000m Declination (2000) arcmin DE2000s Declination (2000) arcsec pm Annual proper motion arcsec e_pm rms uncertainty on pm arcsec pmPA Position angle of proper motion deg Dpm Comparison of our proper motions with LTT proper motions in sense LTT minus ours arcsec DpmPA Comparison of our position angles with LTT position angles in sense LTT minus ours deg Com Comment number=2 The annual proper motions and the position angles are the means of the two values obtained from the plate pairs; 20 LTT stars were common to the overlapped areas mentioned above. For them, the results, indicated by *, correspond to the means of the values obtained from four plates pairs. --- Patricia Bauer CDS 1998 Apr 22 Herbert Wroblewski <hwroblew@das.uchile.cl> J_A+AS_128_457.xml Detailed images and distance measurements for eighteen irregular galaxies in the Canes Venatici cloud. J/A+AS/128/459 J/A+AS/128/459 BV photometry of irregular galaxies Detailed images and distance measurements for eighteen irregular galaxies in the Canes Venatici cloud. L Makarova I Karanchentsev L O Takalo P Heinamaki M Valtonen Astron. Astrophys. Suppl. Ser. 128 457 1998 1998A&AS..128..459M J/A+AS/124/559 : VI photometry of dwarf galaxies (Karanchentsev+ 1997) Galaxies, photometry galaxies: distances and redshifts galaxies: irregular galaxies: stellar content The tables shows the photometry and colour index for the observed galaxy, with the image parameter SHAR. This parameter is a measure of the difference between the observed width of the object and the psf model.
UGC 6782 11 49.0 +23 50 UGC 7131 12 09.1 +30 54 UGC 7356 12 19.1 +47 05 UGC 7559 12 27.1 +37 08 UGC 7599 12 28.5 +37 13 UGC 7605 12 28.7 +35 43 UGC 7639 12 29.9 +47 31 UGC 7698 12 32.9 +31 32 UGCA 290 12 37.3 +38 44 UGCA 292 12 37.3 +83 29 UGC 7866 12 42.1 +38 30 UGC 7949 12 47.0 +36 29 UGC 8024 NGC 4789A 12 54.0 +27 09 K 215 12 55.5 +19 13 UGC 8638 13 39.3 +24 46 UGC 8651 13 40.0 +40 45 UGC 8760 13 50.8 +38 00 UGC 8833 13 54.8 +35 50
*BV Stellar photometry results Gal Galaxy name --- Seq Star number in the galaxy ----- Xpos X coordinate number=1 The XY positions were calculated from the SW corner (X,Y=0,0) of the image, with +X going to east and +Y to north. This corner is the lower-right corner of the image. pix Ypos Y coordinate number=1 The XY positions were calculated from the SW corner (X,Y=0,0) of the image, with +X going to east and +Y to north. This corner is the lower-right corner of the image. pix Vmag V-magnitude mag B-V B-V colour index mag e_Vmag Error in V magnitude mag e_B-V Error in B-V mag SHAR Image parameter SHAR ---- VI Stellar photometry results (only UGC 7131) Gal Galaxy name --- Seq Star number in the galaxy ----- Xpos X coordinate number=1 The XY positions were calculated from the SW corner (X,Y=0,0) of the image, with +X going to east and +Y to north. This corner is the lower-right corner of the image. pix Ypos Y coordinate number=1 The XY positions were calculated from the SW corner (X,Y=0,0) of the image, with +X going to east and +Y to north. This corner is the lower-right corner of the image. pix Vmag V-magnitude mag V-I V-I colour index mag e_Vmag Error in V magnitude mag e_V-I Error in V-I mag SHAR Image parameter SHAR ---- Patricia Bauer CDS 1997 Jul 28 Leo Takalo <takalo@deneb.astro.utu.fi> J_A+AS_128_459.xml Grids of stellar models. VII. From 0.8 to 60M_{sun}_ at Z=0.10 J/A+AS/128/471 J/A+AS/128/471 Grids of stellar models. VII. Grids of stellar models. VII. From 0.8 to 60M_{sun}_ at Z=0.10 N Mowlavi D Schaerer G Meynet P A Bernasconi C Charbonnel A Maeder Astron. Astrophys. Suppl. Ser. 128 471 1998 1998A&AS..128..471M J/A+AS/96/269 : Stellar Models from 0.8 to 120 Msolar (Schaller+, 1992) J/A+AS/98/523 : Grids of stellar models. II. (Schaerer+ 1993) J/A+AS/101/415 : Grids of stellar models III. (Charbonnel+ 1993) J/A+AS/102/339 : Grids of stellar models IV (Schaerer+, 1993) J/A+AS/103/97 : Grids of stellar models V. (Meynet+ 1994) J/A+AS/115/339 : Stellar models VI. (Charbonnel+, 1996) HR diagrams Mass loss Models, evolutionary Hertzsprung-Russell (HR diagram) stars: evolution stars: interiors We present a new grid of stellar models from 0.8 to 60M_{sun}_ at Z=0.10, with mass loss and moderate overshooting, from the zero age main sequence to either the helium flash (low mass stars), the early AGB phase (intermediate-mass stars or the end of carbon burning (massive stars). The calculations are done with opacities provided by Iglesias & Rogers (1993ApJ...412..752I), completed by those of Alexander & Ferguson (1994ApJ...437..879A) at low temperatures. This grid is a homogeneous extension to very high metallicity of the previous grids published by the Geneva group. It is useful for the study of galactic bulges, elliptical galaxies and eventually quasars. Calculations of stars more massive than 60M_{sun}_ are not presented as these objects lose almost their entire mass during their main sequence phase, and are likely to end their life as white dwarfs.
0.8 M, Z=0.1, with overshooting, standard mass loss 0.9 M, Z=0.1, with overshooting, standard mass loss 1.0 M, Z=0.1, with overshooting, standard mass loss 1.25M, Z=0.1, with overshooting, standard mass loss 1.5 M, Z=0.1, with overshooting, standard mass loss 1.7 M, Z=0.1, with overshooting, standard mass loss 2.0 M, Z=0.1, with overshooting, standard mass loss 2.5 M, Z=0.1, with overshooting, standard mass loss 3.0 M, Z=0.1, with overshooting, standard mass loss 4.0 M, Z=0.1, with overshooting, standard mass loss 5.0 M, Z=0.1, with overshooting, standard mass loss 7.0 M, Z=0.1, with overshooting, standard mass loss 9.0 M, Z=0.1, with overshooting, standard mass loss 12.0 M, Z=0.1, with overshooting, standard mass loss 15.0 M, Z=0.1, with overshooting, standard mass loss 20.0 M, Z=0.1, with overshooting, standard mass loss 25.0 M, Z=0.1, with overshooting, standard mass loss 40.0 M, Z=0.1, with overshooting, standard mass loss 60.0 M, Z=0.1, with overshooting, standard mass loss No Number of selected point --- Age Age yr Mass Actual mass in solar masses solMass log(L) log(luminosity) in solar units [solLum] log(Te) log(effective temperature) [K] X H surface abundance (mass fraction) --- Y He surface abundance (mass fraction) --- C12 12C surface abundance (mass fraction) --- C13 13C surface abundance (mass fraction) --- N14 14N surface abundance (mass fraction) --- O16 16O surface abundance (mass fraction) --- O17 17O surface abundance (mass fraction) --- O18 18O surface abundance (mass fraction) --- Ne20 20Ne surface abundance (mass fraction) --- Ne22 22Ne surface abundance (mass fraction) --- QCC Core mass fraction --- log(Tu) log(uncorrected Teff) (WR stars only) [K] log(Mdot) log(mass loss rate) [solMass/yr] log(rho_c) log(central density) [g/cm3] log(Tc) log(central temperature) [K] Xc H central abundance (mass fraction) --- Yc He central abundance (mass fraction) --- C12c 12C central abundance (mass fraction) --- C13c 13C central abundance (mass fraction) --- N14c 14N central abundance (mass fraction) --- O16c 16O central abundance (mass fraction) --- O17c 17O central abundance (mass fraction) --- O18c 18O central abundance (mass fraction) --- Ne20c 20Ne central abundance (mass fraction) --- Ne22c 22Ne central abundance (mass fraction) --- Patricia Bauer CDS 1997 Nov 04 Nami Mowlavi <Nami.Mowlavi@obs.unige.ch> J_A+AS_128_471.xml B[e] stars. V. HD 50138 = MWC 158 J/A+AS/128/475 J/A+AS/128/475 Spectroscopy of MWC 158 B[e] stars. V. HD 50138 = MWC 158 C Jaschek Y Andrillat Astron. Astrophys. Suppl. Ser. 128 475 1998 1998A&AS..128..475J J/A+AS/117/281 : B[e] stars. I. HD 51585 (= OY Gem) (Jaschek+, 1996) J/A+AS/118/495 : B[e] stars. II. MWC 349 A (Andrillat+ 1996) J/A+AS/120/99 : B[e] stars. III. MWC 645 (Jaschek+, 1996) Equivalent widths Spectra, infrared Spectroscopy stars: emission-line, Be stars: individual (HD 50138) stars: peculiar On the basis of spectroscopic CCD material obtained at the Haute Provence Observatory, we provide line identifications and equivalent width measurements in the wavelength region 3738-10232 A of the spectrum of HD 50138 Over two hundred features are identified and a comparison of our results with those of other authors is provided. We also discuss the variability of the lines using equivalent widths and descriptions of the line spectrum. We attribute as a best compromise a spectral type of B 5 III. We conclude that the gaseous shell surrounding the star has a temperature of the order of 10 000K and that its distance to the star is of the order of two stellar radii. We discuss the relation of this star to others previously analyzed and warn against hasty generalizations.
HD 50138 MWC 158 06 51 33.3 -06 58 00
Combined list of lines visible in HD 50138 Lambda Laboratory wavelength number=1 5688 - 5782 Atmospheric band H2O 5878 - 5984 Atmospheric band H2O 6277 - 6305 Atmospheric absorption O2 6472 - 6585 Atmospheric absorption H2O 6717 - 6731 Atmospheric absorption H2O 6964 - 7077 Atmospheric absorption H2O 7186 - 7400 Atmospheric absorption H2O 7866 - 8050 Atmospheric absorption H2O 0.1nm n_Lambda Note on Lambda number=2 *: line visible on spectrogram v, taken in March 96. In this case, no equivalent width is given. ?: uncertainty flag --- Char a/e: absorption or emission characteristic of the line; ed: double emission --- Wide w: wide --- EW Equivalent width of the line 0.1nm --- --- EW2 Second equivalent width (only for lambda=8750.47) 0.1nm n_EW Note on EW number=3 ")": Central line depth. The intensity of the continuum is 1.00. a rough equivalence with equivalent width is W = 3 depth, but this is valid only for weak lines. "w": wide ":": indicates a uncertain value +p : refers to the preceding line +f : refers to the following line --- EW3 ? 0.1nm EW4 ? 0.1nm Ident Line identification of the order element ionization stage and multiplet number number=4 J: Fe II lines listed by Johansson (1978PhS....18..217J), followed by their intensity in Johansson's scale **: probably He I 3885.65, from the ^3^P^0^ series, also present. "Hamann and Persson": Hammann F. and Persson S.E., 1989ApJS...71..931H --- Patricia Bauer CDS 1997 Jul 25 J_A+AS_128_475.xml Library of high-resolution UES echelle spectra of F, G, K and M field dwarf stars J/A+AS/128/485 J/A+AS/128/485 Library of UES spectra late-type stars Library of high-resolution UES echelle spectra of F, G, K and M field dwarf stars D Montes E L Martin Astron. Astrophys. Suppl. Ser. 128 485 1998 1998A&AS..128..485M J/A+AS/123/473 : Late-type star spectra (Montes+ 1997) http://www.ucm.es/OTROS/Astrof/fgkmsl/fgkmsl.html http://www.ucm.es/OTROS/Astrof/fgkmsl/UESfgkmsl.html for FITS spectra Spectroscopy Stars, late-type atlases stars: activity stars: fundamental parameters stars: general stars: late-type We present a library of Utrecht echelle spectrograph (UES) observations of a sample of F, G, K and M field dwarf stars covering the spectral range from 4800{AA} to 10600{AA} with a resolution of 55000. These spectra include some of the spectral lines most widely used as optical and near-infrared indicators of chromospheric activity such as H{beta}, MgI b triplet, NaI D{1}, D{2}, HeI D{3}, H{alpha}, and CaII IRT lines, as well as a large number of photospheric lines which can also be affected by chromospheric activity. The spectra have been compiled with the aim of providing a set of standards observed at high-resolution to be used in the application of the spectral subtraction technique to obtain the active-chromosphere contribution to these lines in chromospherically active single and binary stars. This library can also be used for spectral classification purposes. A digital version with all the spectra is available via ftp and the World Wide Web (WWW) (http://www.ucm.es/OTROS/Astrof/fgkmsl/UESfgkmsl.html) in FITS format.
Summary of WHT/UES observations Run Code for the observing run --- Date Date --- Obs Observer --- CCD CCD Detector --- NbOrder Number of echelle orders --- lambdaC Central wavelength 0.1nm Range Wavelength range covered 0.1nm AA/pixel Range of reciprocal dispersion achieved 0.1nm/pix UES spectral orders (Jul-93) UES spectral orders (Dec-93) UES spectral orders (Apr-94, Mar-95, Jun-95) UES spectral orders (Nov-94) No Order number --- lambdaI Initial wavelength 0.1nm lambdaF Final wavelength 0.1nm Lines Spectral lines of interest --- List of stars, Spectral type and name of the corresponding FITS spectra HD HD number --- HR HR number --- Name name of the star --- SpType Spectral type --- Spectra Original name of FITS file number=1 The original name was made as starname_ues_Run, using the number of the observing run given in table1.dat. This name being too long, it was assigned a shorter name given in column FITSfile. Many spectra are not available. --- fitsFile Name of file found in subdirectory spectra number=1 The original name was made as starname_ues_Run, using the number of the observing run given in table1.dat. This name being too long, it was assigned a shorter name given in column FITSfile. Many spectra are not available. --- RAh Right Ascension 2000 (hours) number=2 the position has beed added from the SIMBAD data-base. h RAm Right Ascension 2000 (minutes) number=2 the position has beed added from the SIMBAD data-base. min RAs Right Ascension 2000 (seconds) number=2 the position has beed added from the SIMBAD data-base. s DE- Declination 2000 (sign) number=2 the position has beed added from the SIMBAD data-base. --- DEd Declination 2000 (degrees) number=2 the position has beed added from the SIMBAD data-base. deg DEm Declination 2000 (minutes) number=2 the position has beed added from the SIMBAD data-base. arcmin figure1a.ps Representative spectral orders for the Dec-93 and Nov-94 observing runs of a K1V star, with the line identification marked figure1b.ps Figure1a continued Patricia Bauer CDS 1998 Mar 13 David Montes <dmg@astrax.fis.ucm.es> J_A+AS_128_485.xml The Hamburg Quasar Survey. II. A first list of 121 quasars J/A+AS/128/507 J/A+AS/128/507 The Hamburg Quasar Survey. II. The Hamburg Quasar Survey. II. A first list of 121 quasars D Engels H -J Hagen L Cordis S Koehler L Wisotzki D Reimers Astron. Astrophys. Suppl. Ser. 128 507 1998 1998A&AS..128..507E J/A+AS/115/235 : The Hamburg/ESO survey for bright QSOs. II. (Reimers+, 1996) Hagen et al., Paper I. 1995A&AS..111..195H Galaxies, spectra QSOs Redshifts quasars: general surveys The Hamburg Quasar Survey is a wide-angle objective prism survey for finding bright QSOs in the northern extragalactic sky (|b|>20{deg}; {delta}>0{deg}). The taking of the prism plates for 567 fields covering this area was completed in 1997. Including direct plates for fields with {delta}> 20{deg} the plate archive contains now 1871 plates. In this paper we present a first list of 121 quasars, which were verified by slit spectroscopy in the years 1986-1991, while experiments to develop efficient selection techniques were made. The sample contains objects with brightnesses 15<=B<=19.5 and redshifts z<=2.8 collected over various parts of the sky, for which objective prism plates were available at that time.
Names, coordinates, redshift, observing dates, B magnitudes and comments Name Object Name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec z Redshift --- ObsDate Observing date "DD/MM/YY" Bmag B magnitude mag spFile Name of file (in this directory) containing the spectrum --- Com Comments --- fig4.ps Quasars spectra fig5.ps Quasars spectra fig6.ps Quasars spectra fig7.ps Quasars spectra fig8.ps Quasars spectra fig9.ps Quasars spectra fig10.ps Quasars spectra fig11.ps Quasars spectra fig12.ps Quasars spectra fig13.ps Quasars spectra fig14.ps Quasars spectra fig15.ps Spectrum of quasar HS 2348+0438 Patricia Bauer CDS Dieter Engels Hamburger Sternwarte 1998 Jun 02 Dieter Engels <dengels@hs.uni-hamburg.de> UNKNOWN UNKNOWN * 16-Jan-1998: First version with 121 quasars. * 02-Jun-1998 (from Dieter Engels): With respect to the printed version the following changes were applied to the tables and figures: The spectrum of the last quasar in table2-4.dat (Table 4 in the paper), HS 2348+0438, was not included in the original Figures. Instead the spectrum of another object, the probable quasar HS 1404+3203, originally not assigned for publication in this paper entered Figure 13. The coordinates of HS 1404+3203 are 14 04 45.5 +32 03 31 (B1950). Its brightness is B=17.8+/-0.1 and the redshift is z=2.4, provided that the strong emission line at 4130 Angstroem is Ly alpha. The spectrum published requires verification. The total number of quasars presented in this paper is now 122. table2-4.dat was updated accordingly and the spectrum of HS 2348+0438 is provided as separate Postscript file. J_A+AS_128_507.xml Physical properties of the ionized gas and brightness distribution in NGC 4736 J/A+AS/128/545 J/A+AS/128/545 NGC 4736 HII regions fluxes Physical properties of the ionized gas and brightness distribution in NGC 4736 I Rodrigues H Dottori J Cepa J Vilchez Astron. Astrophys. Suppl. Ser. 128 545 1998 1998A&AS..128..545R VII/20 : Catalogue of HII Regions (Sharpless 1959) H II regions Spectroscopy galaxies: abundances galaxies: individual (NGC 4736) galaxies: ISM galaxies: spiral galaxies: structure Table 3 gives a catalog of HII region positions, diameters and absolute emission line logarithmic fluxes for NGC 4736. Table 4 gives a catalog of continua logarithmic fluxes adjacent to [OII], H{beta}, [OIII], H{alpha}, [SII] and [SIII] emission lines of NGC 4736 HII regions.
NGC 4736 M 94 12 50.9 +41 07
HII region positions, diameters and absolute emission line logarithmic fluxes (see text). Reg HII Region identification number --- HKNGC4736 Hodge & Kennicut's (1983AJ.....88..296H) identification number (HK NGC 4736 NN) --- Xpos E-W distance from the NGC 4736 nucleus arcsec Ypos N-S distance from the NGC 4736 nucleus arcsec D100 HII region halo diameter arcsec F[OII] [OII]3727+3729 flux mW/m2 FHbeta H{beta} flux mW/m2 F[OIII] [OIII]5007 flux mW/m2 FHalpha H{alpha flux mW/m2 F[SII] [SII]6716+6730 flux mW/m2 F[SIII] [SIII]9070 flux mW/m2 C(Hbeta) H{beta} internal extinction mag WHalpha H{alpha} equivalent width 0.1nm LHbeta H{beta} luminosity 10-7W Notes See Note number=1 a: Neither underlying Balmer absorption nor internal reddening corrections were applied. b: Halo diameter not resolved --- Continua logarithmic fluxes of NGC 4736 HII regions Reg HII Region identification number --- [OII]-C Emission line [OII]-continuum intensity 10-2W/m2/nm Hbeta-C Emission line H{beta}-continuum intensity 10-2W/m2/nm [OIII]-C Emission line [OIII]-continuum intensity 10-2W/m2/nm Halpha-C Emission line H{alpha}-continuum intensity 10-2W/m2/nm [SII]-C Emission line [SII]-continuum intensity 10-2W/m2/nm [SIII]-C Emission line [SIII]-continuum intensity 10-2W/m2/nm Notes See Note number=1 a: Neither underlying Balmer absorption nor internal reddening corrections were applied. --- Patricia Bauer CDS 1997 Sep 04 I. Rodrigues <IRAPUAN@if.ufrgs.br> J_A+AS_128_545.xml Delta-a and Stroemgren photometry of stars in the Renson-catalogue of Ap and Am stars J/A+AS/128/573 J/A+AS/128/573 ubvy{Delta}a photometry of Renson stars Delta-a and Stroemgren photometry of stars in the Renson-catalogue of Ap and Am stars H M Maitzen R Pressberger E Paunzen Astron. Astrophys. Suppl. Ser. 128 573 1998 1998A&AS..128..573M III/162 : General Catalogue of Ap and Am stars (Renson+ 1991) Photometry, uvby Stars, Am Stars, Ap stars: chemically peculiar stars: early-type Results of 131 stars from Renson's (1991, Cat. <III/162>) catalogue of Ap and Am stars observed with the {Delta}-a system are presented. With few exceptions the probability division of Renson for membership in the CP2 group of peculiar stars is nicely reflected by peculiar values of {Delta}-a. Comparison with already available {Delta}-a values yields slightly larger values due to a minor shift in the g_1_ filter sampling the depression. For a description of the {Delta}-a and Stroemgren photometric system, see e.g. <GCPD/75> and <GCPD/04>, respectively.
Comparison of our photometry with the literature RNS Rensons number, as in Cat. <III/162> --- HD HD number (Cat. <III/135>) --- d(b-y) Difference of (b-y)_obs_ to the published values mmag d(m1) Difference of (m1)_obs_ to the published values mmag d(c1) Difference of (c1)_obs_ to the published values mmag Program Stars CP CP class --- Nobs Number of nights --- RNS Rensons number, as in Cat. <III/162> --- HD HD number (Cat. <III/135>) --- Vmag mag(V) from Renson (1991, Cat. <III/162>) mag b-y Observed b-y mmag e_b-y Error of b-y mmag m1 Observed m1 mmag e_m1 Error of m1 mmag c1 Observed c1 mmag e_c1 Error of c1 mmag Da Observed {Delta}a mmag e_Da Error of {Delta}a mmag SpType Spectral type from Renson (1991, Cat. <III/162>) --- Patricia Bauer CDS 1998 Feb 05 Ernst Paunzen <ernst@tycho.ast.univie.ac.at> J_A+AS_128_573.xml A photometric catalogue of galaxies in the cluster Abell 85 J/A+AS/128/67 J/A+AS/128/67 BVR photometry of Abell 85 A photometric catalogue of galaxies in the cluster Abell 85 E Slezak F Durret J Guibert C Lobo Astron. Astrophys. Suppl. Ser. 128 67 1998 1998A&AS..128...67S Clusters, galaxy Galaxies, photometry galaxies: clusters: individual (ABCG 85) galaxies: photometry We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&A...322...53P; Lima-Neto et al., 1997A&A...327...81L).
Catalogue of 4232 galaxies from the SERC-J 681 blue plate No Running number in the catalogue --- RAh Right ascension of the object (equinox 2000.0) h RAm Right ascension of the object (equinox 2000.0) min RAs Right ascension of the object (equinox 2000.0) s DE- Declination sign --- DEd Declination of the object (equinox 2000.0) deg DEm Declination of the object (equinox 2000.0) arcmin DEs Declination of the object (equinox 2000.0) arcsec eps Ellipticity defined as sqrt([1-(b\a)]^2^) --- PA position angle of the major axis (from North to East) deg BJmag B_J_ magnitude mag Vmag V magnitude mag Rmag R magnitude mag Xpos X position number=1 Position relative to the centre defined as that of the diffuse X-ray emission of the cluster (see text) arcsec Ypos Y position number=1 Position relative to the centre defined as that of the diffuse X-ray emission of the cluster (see text) arcsec Name1 Cross-identifications with the list by Malumuth et al. (1992AJ....104..495M) --- Name2 Cross-identifications with the list by Beers et al. (1991AJ....102.1581B) --- Name3 Cross-identifications with the list by Murphy (1984, Cat. <J/MNRAS/211/637>) --- Catalogue of 805 galaxies measured from CCD data No Running number in the catalogue --- RAh Right ascension of the object (equinox 2000.0) h RAm Right ascension of the object (equinox 2000.0) min RAs Right ascension of the object (equinox 2000.0) s DE- Declination sign --- DEd Declination of the object (equinox 2000.0) deg DEm Declination of the object (equinox 2000.0) arcmin DEs Declination of the object (equinox 2000.0) arcsec Rad Isophotal radius arcsec eps Ellipticity e defined as sqrt([1-(b/a)]^2^) --- PA Position angle of the major axis (anticlockwise from North) deg Vmag V magnitude mag Rmag R magnitude mag Xpos X position number=1 Positon relative to the centre assumed to have coordinates: RA = 0h 41mn 51.90s, DE = -9deg 18' 17.0" (equinox 2000.0); this centre was chosen to coincide with that of the diffuse X-ray gas component as defined by Pislar et al. (1997A&A...322...53P). arcsec Ypos Y position number=1 Positon relative to the centre assumed to have coordinates: RA = 0h 41mn 51.90s, DE = -9deg 18' 17.0" (equinox 2000.0); this centre was chosen to coincide with that of the diffuse X-ray gas component as defined by Pislar et al. (1997A&A...322...53P). arcsec Patricia Bauer CDS 1997 Jun 13 Eric Slezak, <slezak@purcell.obs-nice.fr> J_A+AS_128_67.xml Radiative transition probabilities for forbidden lines in singly ionized cobalt (Co II) J/A+AS/129/147 J/A+AS/129/147 Co II radiative transition probabilities Radiative transition probabilities for forbidden lines in singly ionized cobalt (Co II) P Quinet Astron. Astrophys. Suppl. Ser. 129 147 1998 1998A&AS..129..147Q Atomic physics atomic data supernovae: general Radiative transition probabilities have been calculated for the magnetic dipole (M1) and electric quadrupole (E2) transitions connecting the 47 metastable energy levels in the 3d^8^, 3d^7^ 4s and 3d^6^ 4s^2^ configurations in Co II. The most important configuration interaction (CI) and relativistic effects have been taken into account in the computations carried out with the help of the relativistic Hartree-Fock (HFR) method combined with a semi-empirical optimization of the radial parameters.
Radiative transition probabilities, Aki in s-1, as calculated in the present work for forbidden lines of Co II. Multiplet Multiplet --- J-J' J-J' --- Lambda Predicted wavelengths from observed energy levels number=1 Wavelengths, in air, are deduced from the observed energy levels compiled by Sugar & Corliss (1985, J. Phys. Chem. Ref. Data 14, Suppl. 2) 0.1nm Type Type of transition --- Aki Transition probabilities number=2 Only transitions for which Aki is greater than 0.001 s-1 are reported. s-1 Comm Comment on the A-value number=3 * Cancellation effects present. --- Patricia Bauer CDS 1997 Dec 05 Pascal Quinet <Pascal.Quinet@umh.ac.be> J_A+AS_129_147.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest XVIII: Si XI and Si XIII spectral lines J/A+AS/129/155 J/A+AS/129/155 Si XI & Si XIII lines Stark broadening Stark broadening of spectral lines of multicharged ions of astrophysical interest XVIII: Si XI and Si XIII spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 129 155 1998 1998A&AS..129..155D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines J/A+AS/127/295 : Stark broadening of Kr II lines J/A+AS/127/543 : Stark broadening of S V lines J/A+AS/128/203 : Stark broadening of Mn, Ga & Ge multiplets Atomic physics atomic data line: profiles plasmas Using a semiclassical perturbation approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 Si XI multiplets for perturber densities 10^18^-10^23^cm^-3^ and temperatures T=500000-4000000K, and for 61 Si XIII multiplets for perturber densities 10^16^-10^23^cm^-3^ and temperatures T=500000-6000000K. For lower perturber densities, obtained results are linear with perturber density.
Stark broadening parameters due to e-, p- and He III-impacts for Si XI and Si XIII N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ (4) --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ (4) --- dHe++ shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1997 Sep 09 Dr Milan Dimitrijevic <mdimitrijevic@aob.bg.ac.yu> J_A+AS_129_155.xml GRANAT/WATCH catalogue of cosmic gamma-ray bursts: December 1989 to September 1994 J/A+AS/129/1 J/A+AS/129/1 GRANAT/WATCH catalogue of gamma-ray bursts GRANAT/WATCH catalogue of cosmic gamma-ray bursts: December 1989 to September 1994 S Y Sazonov R A Sunyaev O V Terekhov N Lund S Brandt A J Castro-Tirado Astron. Astrophys. Suppl. Ser. 129 1 1998 1998A&AS..129....1S Atlases Gamma rays astronomical data bases: miscellaneous catalogs gamma rays: bursts We present the catalogue of gamma-ray bursts (GRB) observed with the WATCH all-sky monitor on board the GRANAT satellite during the period December 1989 to September 1994. The cosmic origin of 95 bursts comprising the catalogue is confirmed either by their localisation with WATCH or by their detection with other GRB experiments. For each burst its time history and information on its intensity in the two energy ranges 8-20keV and 20-60keV are presented. Most events show hardening of the energy spectrum near the burst peak. In part of the bursts an X-ray precursor or a tail is seen at 8-20keV. We have determined the celestial positions of the sources of 47 bursts. Their localisation regions (at 3-sigma confidence level) are equivalent in area to circles with radii ranging from 0.2 to 1.6deg. The burst sources appear isotropically distributed on the sky on large angular scales.
GRANAT
Basic information on GRANAT/WATCH gamma-ray bursts GRB Burst name, includes date (YYMMDD) --- Th Start time (hours) h Tm Start time (minutes) min Ts Start time (seconds) s T90 Duration s e_T90 Uncertainty on duration s Lflu 8-20 keV fluence 10-14J/cm2 e_Lflu Uncertainty on 8-20 keV fluence 10-14J/cm2 Hflu 20-60 keV fluence 10-14J/cm2 e_Hflu Uncertainty on 20-60 keV fluence 10-14J/cm2 HR Hardness ratio (20-60/8-20) --- e_HR Uncertainty on hardness ratio --- Lpeak 8-20 keV peak flux 10-7mW/m2 e_Lpeak Uncertainty on 8-20 keV peak flux 10-7mW/m2 Hpeak 20-60 keV peak flux 10-7mW/m2 e_Hpeak Uncertainty on 20-60 keV peak flux 10-7mW/m2 Rem Remarks, see Note number=1 a = Direction of burst arrival unknown b = Burst superimposed on variable background. Values given for the parameters possibly in error c = Burst source was either outside or at the border of the WATCH field of view according to the BATSE localisation --- Confirm Confirmations, see Note number=2 Bursts were also observed by other instruments. Codes for the instruments: B = BATSE/CGRO C = COMPTEL/CGRO D = DMS E = WATCH/EURECA G = GINGA K = KONUS/GRANAT M = Mars Observer O = OSSE/CGRO P = PVO Ph = PHEBUS/GRANAT S = SIGMA/GRANAT U = ULYSSES Y = YOHKOH --- Patricia Bauer CDS 1997 Aug 25 Sergei Sazonov <ss@hea.iki.rssi.ru> J_A+AS_129_1.xml Abundances of metal-rich stars. Detailed abundance analysis of 47 G and K dwarf stars with [Me/H] > 0.10 dex. J/A+AS/129/237 J/A+AS/129/237 G and K dwarfs abundances Abundances of metal-rich stars. Detailed abundance analysis of 47 G and K dwarf stars with [Me/H] > 0.10 dex. S Feltzing B Gustafsson Astron. Astrophys. Suppl. Ser. 129 237 1998 1998A&AS..129..237F J/A+AS/102/603 : Chemical evolution of the galactic disk II. (Edvardsson+ 1993) Barbuy & Grenon, 1990, in: ESO/CTIO Workshop on Bulges of Galaxies, La Serena, Chile, Jan. 16-19, 1990, Proceedings (A92-18101 05-90). Garching, Federal Republic of Germany, European Southern Observatory, 1990, p. 83-86; Discussion, p. 86, 87. Abundances Stars, dwarfs galaxies: fundamental parameters Galaxy: abundances Galaxy: evolution stars: abundances stars: late-type The table presents the abundances of all 47 dwarf stars analysed in the paper. We give abundances relative to the Sun in the standard notation of [X/H]=log(X/H)_star_-log(X/H)_{sun}_. The 5 K dwarf stars and 3 stars in common with Barbuy & Grenon (1990) appear at the end of the table. The label of each column indicates the ion the quoted abundances are derived from. For each star we give the abundance, [X/H], the line-to-line scatter (if more than one line is used) and the number of lines used. The stars are ordered in the same way as in Table 1 in the paper, ie. the K dwarf stars and the stars in common with Barbuy & Grenon (1990) are found at the end.
Elemental abundances HD HD (Cat. <III/135>) number --- m_HD Multiplicity index on HD --- Ion Ion designation --- [X/H] Abundance (log(X/H)_star-log(X/H)_{sun}_) [Sun] Sc Line-to-line scatter --- Nline Number of lines --- Star positions (from Simbad database) HD HD (Cat. >III/135>) number --- m_HD Multiplicity index on HD --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Patricia Bauer CDS 1998 Apr 27 Sofia Feltzing <sofia@ast.cam.ac.uk> J_A+AS_129_237.xml A catalogue of velocities in the cluster of galaxies Abell 85 J/A+AS/129/281 J/A+AS/129/281 ABCG 85 velocities catalogue A catalogue of velocities in the cluster of galaxies Abell 85 F Durret P Felenbok C Lobo E Slezak Astron. Astrophys. Suppl. Ser. 129 281 1998 1998A&AS..129..281D J/A+AS/128/67 : BVR photometry of Abell 85 (Slezak+ 1998) Clusters, galaxy Photometry Radial velocities Redshifts galaxies: clusters: individual (ABCG 85) galaxies: distances and redshifts instrumentation: spectrographs We present a catalogue of velocities for 551 galaxies (and give the coordinates of 39 stars misclassified as galaxies in our photometric plate catalogue) in a region covering about 100'x100' (0.94x0.94Mpc for an average redshift of 0.0555, assuming H_0_=50km/s/Mpc) in the direction of the rich cluster ABCG85. This catalogue includes previously published redshifts by Beers et al. (1991AJ....102.1581B) and Malumuth et al. (1992AJ....104..495M), together with our 367 new measurements. A total of 305 galaxies have velocities in the interval 13350-20000km/s, and will be considered as members of the cluster. ABCG 85 therefore becomes one of the clusters with the highest number of measured redshifts; its optical properties are being investigated in a companion paper.
Velocity catalogue for 551 galaxies in the direction of the cluster of galaxies ABCG 85 Seq Running number --- RAh Right ascension (equinox 2000.0) h RAm Right ascension (equinox 2000.0) min RAs Right ascension (equinox 2000.0) s DE- Declination sign --- DEd Declination (equinox 2000.0) deg DEm Declination (equinox 2000.0) arcmin DEs Declination (equinox 2000.0) arcsec cz Velocity km/s e_cz Error on velocity km/s R Tonry & Davis (1979AJ.....84.1511T) R parameter --- A/E 0 = absorption, 1 = emission velocity --- q_cz Quality number=1 1 = best, 3 = worst, 0 = literature --- r_cz Origin number=2 1 = Malumuth et al., 1992AJ....104..495M 2 = Beers et al., 1991AJ....102.1581B 3 = our data --- Xpos Right ascension relative to center arcsec Ypos Declination relative to center arcsec Dist Distance to center arcsec bJmag b_J photographic plate magnitude mag Vmag V magnitude mag Rmag R magnitude mag Ref Reference to Beers (B), Malumuth (M), and galaxies D, I, K, H, SW and cD in Pislar et al. (1997A&A...322...53P). --- Patricia Bauer CDS 1997 Nov 25 Florence Durret <durret@iap.fr> J_A+AS_129_281.xml Long-term visual spectrophotometric behaviour of Be stars J/A+AS/129/289 J/A+AS/129/289 Long-term spectrophotometry of Be stars Long-term visual spectrophotometric behaviour of Be stars A Moujtahid J Zorec Astron. Astrophys. Suppl. Ser. 129 289 1998 1998A&AS..129..289M III/187 : Classification of stars in BCD (Barbier/Chalonge/Divan) Spectrophotometry Stars, Be stars: Be stars: spectrophotometry stars: variables: general The long-term spectrophotometric variations of 49 Be stars are studied using the U and V magnitudes of the UBV system, the total Balmer discontinuity D and the visible gradient {Phi}_rb_. BCD (Barbier-Chalonge-Divan, see Chalonge & Divan, 1952AnAp...15..201C) spectrophotometric and photometric data in five different photometric systems, obtained in most cases since 1950 and reduced to the BCD system, were used. The (U,D), (V,D), ({Phi}_rb_,D) and ({Phi}_rb_,V) correlations obtained differ from star to star and they can be single or double-valued. They differ clearly for Be phases or Be-shell phases. Be stars with small V.sin(i) showing the "spectrophotometric shell behaviour": D>D*, were found. This finding implies either that strongly flattened models of circumstellar envelopes are in doubt for these stars, or that not all Be stars are rapid rotators. Comparison of observed variations with those predicted for model Be stars with spherical circumstellar envelopes of variable densities and dimensions implies that spectrophotometric patterns of Be phases are due to circumstellar envelopes in low opacity regimes, while those of spectrophotometric shell phases are due to circumstellar envelopes in high opacity regimes. In a given star, the envelope regions responsible for the observed variations of D and {Phi}_rb_ in spectrophotometric shell phases seem to be smaller and denser than those producing the observed variations of these parameters in spectrophotometric Be phases. The high positive RV found in strong shell phases might favor the formation of compact circumstellar layers near the star.
Star positions (from Simbad database) HD HD (Cat. <III/135>) number --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec The studied Be stars HD HD (Cat. <III/145>) number --- HR HR (Cat. <V/50>) number --- Name Other name --- SpType Spectral type --- n_SpType Note on spectral type number=1 An a indicates spectral classification form the BCD system. Otherwise, it is taken from the Hipparcos Input Catalogue (Turon et al. 1992, Cat. <I/196>), Buscombe (1977, 1980, 1981, 1988, See Cat. <III/189>), Hubert-Delplace & Hubert (1979, An Atlas of Be Stars, Obs. de Paris-Meudon and Obs. de Haute-Provence), Sletteback (1982ApJS...50...55S), the Bright Star Catalogue (Cat. <V/50>), and Supplement (Cat. <V/36>) --- FigFile Figure name in subdirectory fig --- Dstar Stellar Balmer discontinuity magnitude mag u_Dstar Uncertainty flag on Dstar --- n_Dstar Note on Dstar number=2 An a indicates BCD values of Dstar, otherwise Dstar is the mean value for the adopted MK spectral classification. --- <Vmag> Average V magnitude mag e_<Vmag> rms uncertainty on <Vmag> mag <Dmag> Average total Balmer discontinuity magnitude mag e_<Dmag> rms uncertainty on <Dmag> mag <Phirb> Average visible gradient mag e_<Phirb> rms uncertainty on <Phirb> mag JDf First observation date (-2400000) --- n_JDf Dash --- JDl Last observation date (-2400000) --- N Number of individual triads (Vmag, Dmag, Phirb) --- Ref References detailed in file refs.dat --- References of table1.dat Ref Reference number --- BibCode Simbad bibcode --- Aut Author name, and comments --- Patricia Bauer CDS 1998 Apr 20 Ali Moujtahid <Ali.Moujtahid@obspm.fr> J_A+AS_129_289.xml On the morphology of peculiar ring galaxies. J/A+AS/129/357 J/A+AS/129/357 Morphology of peculiar ring galaxies On the morphology of peculiar ring galaxies. M Faundez-Abans M de Oliveira-Abans Astron. Astrophys. Suppl. Ser. 129 357 1998 1998A&AS..129..357F VII/170 : Catalogue of Southern Peculiar Galaxies and Associations (Arp+, 1987) Galaxies, ring Morphology galaxies: fundamental parameters galaxies: peculiar galaxies: structure It is proposed that Peculiar Ring Galaxies can be divided into five principal types according to the morphology of the ring and bulge, based on the visual inspection of 489 selected object. Those objects have been named "peculiar" following the "Catalogue of Southern Peculiar Galaxies and Associations" by Arp & Madore (1986, Cat. <VII/170>).
List of galaxies Object Object name --- OName Other designation --- RAh Right ascension 2000 (hours) h RAm Right ascension 2000 (minutes) min RAs Right ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes of arc) arcmin DEs Declination 2000 (seconds of arc) arcsec MType Ring Family number=1 P = Polar HL = Hoag E = Elliptcial (the warped behavior is often present) I = Irregular CS = Centrally Smooth N = Normal Ring Galaxy r? = probably ringed s = spiral (blank) = not classified --- Ba Bulge's major axis (seconds of arc) arcsec u_Ba Uncertainty flag on Ba --- Bb Bulge's minor axis (seconds of arc) arcsec u_Bb Uncertainty flag on Bb --- Ra Ring's major axis (seconds of arc) arcsec u_Ra Uncertainty flag on Ra --- Rb Ring's minor axis (seconds of arc) arcsec u_Rb Uncertainty flag on Rb --- NotNum Note running number (see appena file) --- Notes to Table 2 NotNum Note number for Object (see table2) --- Text Text of Notes on Objects of table2 --- M. Faundez-Abans ? 1997 Nov 14 Mariangela de Oliveira-Abans <mabans@lna.br> J_A+AS_129_357.xml The ESO Nearby Abell Cluster Survey. V. The catalogue: contents and instructions for use J/A+AS/129/399 J/A+AS/129/399 The ENACS Catalogue. V. The ESO Nearby Abell Cluster Survey. V. The catalogue: contents and instructions for use P Katgert A Mazure R den Hartog C Adami A Biviano J Perea Astron. Astrophys. Suppl. Ser. 129 399 1998 1998A&AS..129..399K J/A+A/310/8 : The ESO Nearby Abell Cluster Survey I. (Katgert+, 1996) J/A+A/310/31 : The ESO Nearby Abell Cluster Survey II. (Mazure+ 1996) Biviano et al., Paper III. 1997A&A...321...84B Adami et al., Paper IV. 1998A&A...331..493A Clusters, galaxy Magnitudes Redshifts catalogs galaxies: clusters: general galaxies: distances and redshifts galaxies: photometry Table enacs presents the full ENACS catalogue: i.e. redshifts and photometry of 5634 galaxies in the directions of 107 rich Southern cluster candidates from the ACO catalogue. Table 2 of this paper lists additional redshifts from the literature for 33 galaxies contained within the Optopus areas of 4 clusters observed in the ENACS. Table 5 of this paper lists the centre of the Optopus plates and the dates of the Optopus observations We present the catalogue resulting from the ESO Nearby Abell Cluster Survey (the ENACS), which contains redshifts and magnitudes for 5634 galaxies in the directions of 107 rich, nearby southern Abell cluster candidates. We describe the contents of the catalogue and discuss the results of a comparison between the ENACS catalogue and the COSMOS Galaxy Catalogue. When cross-correlating the two catalogues we find that, at least in the areas of the ENACS clusters, the completeness of the COSMOS catalogue is somewhat lower than was estimated previously for the carefully analyzed and well-calibrated part of the COSMOS catalogue known as the Edinburgh-Durham Southern Galaxy Survey (EDSGC). The galaxy positions in the COSMOS and ENACS catalogues are found to be on the same system to within about one arcsecond. For the clusters for which the photometry in the ENACS and COSMOS catalogues is based on the same survey plates, the two magnitude scales agree very well. We confirm that the photometric calibration in the EDSGC subset of the COSMOS catalogue is of higher quality than in the EDSGC complement. The ENACS galaxy samples are unbiased subsets of the COSMOS catalogue as far as the projected galaxy distribution is concerned, except in only a few cases. We summarize how the ENACS galaxy samples are subsets of the COSMOS catalogues in the ENACS apertures, with respect to magnitude. For the ENACS catalogue as a whole, we describe the apparent incompleteness at faint magnitudes and towards higher redshifts. Finally, we provide some detailed information about the ENACS catalogue that is essential for its proper statistical use and we summarize some facts that must be remembered when selecting subsets of galaxies from it. Objects:
The ENACS catalogue ACO ACO (Cat. <VII/4>) number of the target cluster --- Seq Sequence number of galaxy in cluster survey (total number of redshifts in the survey) --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Rmag25 R-band magnitude within 25th mag/arcsec^2^ number=1 A value of 0.00 means not available mag cz Adopted heliocentric velocity of galaxy km/s e_cz Estimated error in adopted velocity km/s czabs Heliocentric velocity from absorption lines number=1 A value of 0.00 means not available km/s R R-parameter of cross-correlation (Tonry & Davis, 1979AJ.....84.1511T) number=1 A value of 0.00 means not available --- czemi Heliocentric velocity from emission lines number=1 A value of 0.00 means not available km/s LC Emission line code number=2 0: no emission lines seen 1: OII {lambda} 3727 2: H{beta} 3: OII {lambda} 3727 + H{beta} 4: OIII {lambda} 4959/5007 5: OII {lambda} 3727 + OIII {lambda} 4959/5007 6: H{beta} + OIII {lambda} 4959/5007 7: OII {lambda} 3727 + H{beta} + OIII {lambda} 4959/5007 --- EC Excitation code number=3 0: not available 1: H{beta} > OIII {lambda} 5007 2: OIII {lambda} 5007 > H{beta} > OIII {lambda} 4959 3: H{beta} ~ OIII {lambda} 4959 4: H{beta} < OIII {lambda} 4959 5: AGN (i.e.: very broad H{beta}) --- CI Continuum index number=4 Not given for spectra without emission lines 0: not available 1: featureless 2: metallic absorption lines 3: strong absorption under H{beta} --- Additional Redshifts for Galaxies in the Optopus Areas ACO Number (Cat. <VII/4>) of the target cluster --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Rmag25 R-band magnitude within 25th mag/arcsec^2^ mag cz Adopted heliocentric velocity of galaxy km/s e_cz Estimated error in adopted velocity km/s Ref Reference to literature source number=1 1: Zabludoff et al., 1993, Cat. <J/AJ/106/1273> 2: Huchra et al., 1995, Cat. <VII/193> 3: Faber et al. 1977AJ.....82..187F 4: Beers et al., 1991AJ....102.1581B 5: Hill et al., 1993, Cat. <J/AJ/106/831> 6: Malumuth et al., 1992AJ....104..495M 7: Quintana et al., 1985AJ.....90..410Q --- Centres of Optopus Plates and Optopus Observing Dates ACO Number of the target cluster --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Date Observing date "DD/MM/YY" Francois Ochsenbein CDS 1998 Apr 20 Peter Katgert <katgert@strw.leidenuniv.nl> J_A+AS_129_399.xml Fe I line shifts in the optical spectrum of the Sun J/A+AS/129/41 J/A+AS/129/41 Fe I line shifts in the Sun Fe I line shifts in the optical spectrum of the Sun C Allende Prieto R J Garcia Lopez Astron. Astrophys. Suppl. Ser. 129 41 1998 1998A&AS..129...41A J/A+AS/102/269 : Lab. and solar Highly-excited levels of Fe I (Nave+ 1993) J/ApJS/94/221 : New multiplet table for FeI (Nave+, 1994) Atomic physics Sun atlases convection stars: atmospheres Sun: photosphere Central wavelengths measured in the FTS disc-centre spectrum, in the FTS flux spectrum, rest wavelengths, excitation potentials, transition probabilities (log(gfs)) and line equivalent widths at the centre of the disc when available (from Moore et al. 1966 (The Solar Spectrum 2935{AA} to 8770{AA}, National Bureau of Standards Monograph 61) and compiled by A. D. Wittmann, private communication). An asterisk in the equivalent width means that the line has a blend.
Caption of the table Int. Central Waveleng. in the disc-centre spectrum 0.1nm Flux Central Wavelengths in the flux spectrum 0.1nm Lab Central Wavelengths at rest (Nave et al., 1994, Cat. <J/ApJS/94/221>) 0.1nm EP Excitation potential (Thevenin, 1989A&AS...77..137T, 1990A&AS...82..179T) eV log(gf) Transition probabilities (Nave et al. 1994, Cat. <J/ApJS/94/221>) --- EW Equivalent widths (disc centre) mA n_EW Note on line number=1 *: The line is Known to be blended --- Patricia Bauer CDS 1997 Sep 18 Carlos Allende Prieto <callende@ll.iac.es> J_A+AS_129_41.xml Determination of the temperatures of selected ISO flux calibration stars using the Infrared Flux Method J/A+AS/129/505 J/A+AS/129/505 Effective temperatures by Infrared Flux Method Determination of the temperatures of selected ISO flux calibration stars using the Infrared Flux Method D E Blackwell A E Lynas-Gray Astron. Astrophys. Suppl. Ser. 129 505 1998 1998A&AS..129..505B Effective temperatures Photometry, infrared stars: fundamental parameters stars: temperatures Effective temperatures for 420 stars with spectral types between A0 and K3, and luminosity classes between II and V, selected for a flux calibration of the Infrared Space Observatory, ISO, have been determined using the Infrared Flux Method (IRFM). The determinations are based on narrow and wide band photometric data obtained for this purpose, and take into account previously published narrow-band measures of temperature.
Total fluxes and derived temperatures for ISO Stars HD HD number --- Flux Integrated stellar flux nW/m2 T Derived stellar temperature K r_Flux Source of infrared data number=1 A: Telescopio Carlos Sanchez (TCS) data B: ESO data --- e_T Estimated probable errors of derived temperatures % Patricia Bauer CDS 1998 Aug 11 UNKNOWN UNKNOWN From A&AS electronic version J_A+AS_129_505.xml High resolution spectroscopy of the post-red supergiant IRC +10420. I: The data. J/A+AS/129/541 J/A+AS/129/541 Spectroscopy of IRC +10420 High resolution spectroscopy of the post-red supergiant IRC +10420. I: The data. R D Oudmaijer Astron. Astrophys. Suppl. Ser. 129 541 1998 1998A&AS..129..541O Spectra, infrared Spectroscopy Stars, supergiant circumstellar matter stars: AGB and post-AGB stars: emission-line, Be stars: individual (IRC+10 420) supergiants A high resolution optical spectrum of the post-red supergiant candidate IRC +10420 is presented. The Utrecht Echelle Spectrograph observations, with a total integration time of more than 9 hours provide a spectral coverage from 3850 A to 1micron, and a spectral resolution of 9km/s. The spectrum is shown, and an identification list of lines in the spectrum is provided. From a preliminary analysis of the spectrum we find that the spectral type of IRC+10420 has changed from F8I+ in 1973 to mid- to early A type now, confirming the results of Oudmaijer et al. (1996MNRAS.280.1062O), who claimed a change in temperature based on photometric changes. It is shown that most of the emission lines in the spectrum of IRC +10420 are blue-shifted with respect to the systemic velocity traced by circumstellar rotational CO emission, while the (few) absorption lines - with the exception of some high excitation lines - are red-shifted by 25km/s, which may suggest infall of material onto the star. Finally, it is found that the interstellar extinction towards IRC +10420, as traced by the Diffuse Interstellar Bands is very large, with an inferred E(B-V) of 1.4+/-0.5 compared to a total E(B-V) of 2.4. This table provides the line identifications for the measured spectral lines from atomic species. Listed in the table are respectively the laboratory wavelength (in air) taken from Moore (1945, in A multiplet table of astrophysical interest, Contribution from the Princeton University Observatory No. 20.), the line identification (ion and multiplet), the energies of the lower levels of the transitions in eV, and the log(gf). The latter two values are taken from Wiese et al. (1966, Nat. Stand. Ref. Data Ser. 20 and 1969, Nat. Stand. Ref. Data Ser. 22), Martin et al. (1988, Cat. <VI/72>) and Fuhr et al. (1988, Cat. <VI/72>). The spectral lines that are marked `UN' were not identified, the wavelength given for these lines is the observed wavelength. Then next entries in the table are the velocity shift of the centres of spectral lines (in LSR), the equivalent width in milli-Angstrom, and the full-width-at-half maximum of the fit in Angstrom. The velocity shifts have been measured by fitting Gaussian profiles through the lines, the equivalent widths have been measured by integrating the line over the continuum. In the case of overlapping lines, the lines were de-composed by fitting multiple Gaussian components to the profiles. In these cases (marked with `deb.' in the table) the equivalent widths are the areas under the Gaussian fits. Equivalent widths for lines that could not be deblended, are given between brackets. These values represent the total equivalent width of the lines concerned.
IRC+10420 19 24 26.7 +11 15 11
Spectroscopy of IRC +10420, line identifications W Air wavelength 0.1nm El Ion (UN = unidentified lines) -- Mult Multiplet -- Chil Lower level excitation energy eV loggf log(gf) -- Vlsr Velocity shift of the centre of spectral lines (in Local Standard of Rest) number=1 Estimated accuracy of central velocities is 5km/s km/s EW Equivalent Width number=2 Error in EW is mostly 10% 10-4nm n_EW Note on EW number=4 ':' : EW especially uncertain ')' : lines that could not be deblended. The value represents the total equivalent width of the lines concerned 'a' : absorption 'e' : emission --- FWHM Full-Width-Half-Maximum number=3 Error FWHM is 10% 0.1nm Rem Remarks number=5 Users should take special care interpreting line EW and FWHM in cases where these were measured through a de-blending routine. The lines are marked with `deb' -------------------------------------------------------------------------------- Acknowledgements: Rene Oudmaijer <r.oudmaijer@ic.ac.uk> -- Patricia Bauer CDS 1997 Dec 19 J_A+AS_129_541.xml Elemental abundance analyses with Complejo Astronomico El Leoncito REOSC Echelle Sprectrograms. III. HR 4487, 14 Hydrae and 3 Centauri A J/A+AS/129/563 J/A+AS/129/563 Abundances of HR 4487, 14 Hyd and 3 Cen A Elemental abundance analyses with Complejo Astronomico El Leoncito REOSC Echelle Sprectrograms. III. HR 4487, 14 Hydrae and 3 Centauri A O I Pintado S J Adelman A F Gulliver Astron. Astrophys. Suppl. Ser. 129 563 1998 1998A&AS..129..563P J/A+AS/125/219 : Abundances of mu Lep, 7 Sex, HR 4817 + 28 Her (Adelman+ 1997) Pintado & Adelman, Paper I. (kappa Cnc, HR 7245, xi} Oct) 1996A&AS..118..283P Abundances, peculiar Stars, peculiar stars: abundances stars: chemically peculiar stars: individual (HR 4487, 14 Hya, 3 Cen A) Ussing CASLEO echelle spectrograms, elemental abundances are derived for the sharp-lined non-magnetic CP stars HR 4487, 14 Hya and 3 Cen A. The first two stars are members of the Mercury-Manganese subgroup and have abundances which are similar to other such peculiar stars. The third is a hotter related star. The detection of Mn II lines in its spectrum adds to this relationship.
HR 4487 HD 101189 11 38 07.7 -61 49 35 HD 75333 14 Hya HR 3500 08 49 21.7 -03 26 34 HR 5210 3 Cen A HD 120709 13 51 49.6 -32 59 37
Atomic abundances Name Star name --- Ion Ion --- Nline Number of lines --- Element Element (identical to bytes 9-10) --- log(Nel/Ntot) Derived abundance of Element (ratio of number of atoms to the total number of atoms per unit volume) --- e_log(Nel/Ntot) rms uncertainty on log(Nel/Ntot) --- u_e_log(Nel/Ntot) Uncertainty flag on e_log(Nel/Ntot) --- Elemental abundances of HR 4487, 14 Hya, and 3 Cen A Name Star name --- Ion Ion --- Mult Multiplet number --- lambda Wavelength 0.1nm log(gf) Oscilator strength --- r_log(gf) Reference for log(gf) number=1 BG = Biemont et al. (1981ApJ...248..867B) FW = Fuhr & Wiese (1990, in Lide, D. R. ed, CRC Handbook of Chemistry and Physics, CRC Press, Cleveland, OH) GB = Grevesse et al. (1981, in Upper Main Seq. Chem. Pec. Stars., 23rd Liege 81, P. 211) HL = Hannaford et al. (1982ApJ...261..736H) JS = Jugaku et al. (1961ApJ...134..783J) KX : Kurucz, 1995, in Astrophysical Applications of Powerful New Databases, eds. S. J. Adelman and W. L. Wiese (ASP, San Francisco), ASP Conf. Ser. 78, 205 LA = Lanz & Artru (1985, 1985, Phys. Scripta, 32, 155) LD = Lawler & Dakin (1989, JOSA B, 6, 1457) MF : Martin et al., 1988, J. Phys. Chem. Ref. Data 15, Suppl. 3 and Fuhr et al. 1988, J. Phys. Chem. Ref. Data 15, Suppl. 4 WF : Wiese et al., 1996, J. Phys. Chem. Ref. Data, Monograph 6 WM = Wiese & Martin, 1980, NSRDS-NBS 68. Part 2, US Government Printing Office, Washington, DC. WS : Wiese et al., 1966, NSRDS-NBS 4, US Government Printing, Office, Washington, DC and 1969, NSRDS-NBS, Washington, D.C., US Department of Commerce, National Bureau of Standards --- EW Equivalent width 10-4nm log(N/Ntot) Derived abundance in relative number of atoms --- table3.tex LaTeX version of table3.dat and abund.dat Patricia Bauer CDS 1997 Dec 15 Olga Ines Pintado <opintado@tucbbs.com.ar> J_A+AS_129_563.xml Microvariability of the blazar OJ 287 J/A+AS/129/569 J/A+AS/129/569 BVRI photometry of OJ 287 Microvariability of the blazar OJ 287 G -B Jia X -F Cen H -Y Ma J -C Wang Astron. Astrophys. Suppl. Ser. 129 569 1998 1998A&AS..129..569J J/A+AS/128/315 : BVRI photometry of blazars (JiaGuibin+ 1998) BL Lac objects Photometry, CCD Photometry, UBVRI BL Lacertae objects: individual (OJ 287) galaxies: active Results of BVRI CCD photometric monitoring and fast photometry in the I band for the blazar OJ 287 in 1994-1995 are presented. The predicted outburst of the blazar had been observed, the maximum appeared in 1994 November, after that, the luminosity decreased by 1.6mag for about three months and dropped to near the level in 1994 April. Rapid variations with timescales of minutes, hours and one day were observed in our observations, with small amplitude. The amplitude of the most rapid variations (minutes) is in the range of 0.043-0.12mag . The results of the statistical analysis of the fast photometry data are as follows. In five nights out of six rapid variability appeared in the sampling interval, which ranged from 3.4 minutes to 6.5 minutes, with a rms amplitude of flux variations of 1.70%-2.3%. The rapid variability can be explained by the model of shocks within turbulent jet or of vortices and magnetic flux tubes on accretion disk.
OJ 287 QSO 0851+202 08 54 48.9 +20 06 31
Results for OJ 287 Date Observation date "DD/MM/YY" JD Julian date d Band The observed waveband --- mag Magnitude (BVRI) in the band mag e_mag Error on mag mag Patricia Bauer CDS 1997 Dec 09 Jiancheng Wang <jcwang@public.km.yn.cn> J_A+AS_129_569.xml Monitoring of AO 0235+164 during a faint state J/A+AS/129/577 J/A+AS/129/577 AO 0235+164 BVRI photometry Monitoring of AO 0235+164 during a faint state L O Takalo A Sillanpaa E Valtaoja S Katajainen K Nilsson T Pursimo P Heinamaki M Villata C M Raiteri G Ghisellini G De Francesco L Lanteri M Chiaberge A Peila P Boltwood G Tosti M Fiorucci H Terasranta M Tornikoski P Teerikorpi Astron. Astrophys. Suppl. Ser. 129 577 1998 1998A&AS..129..577T BL Lac objects Photometry, UBVRI BL Lacertae objects: general BL Lacertae objects: individual (AO 0235+164) gravitaional lensing We present the results of the optical and radio monitoring of the BL Lac object AO 0235+164 during a faint state. In both optical and radio bands the source has been observed at the faintest ever recorded levels, reaching V=19.80 and F_22GHz_=0.34Jy. In the optical bands we still see variability with amplitudes up to 1.5 magnitudes on timescales from days to weeks. The radio variability is less dramatic, but in general follows the optical behaviour. A correlation between general trends in the optical and radio behaviour of AO 0235+164 may be recognized in the data from the present monitoring as well as in the historical light curves, suggesting a `base' mechanism responsible for the emission at both frequencies. A good candidate is a synchrotron process in the relativistic jet. Optical flares with no corresponding radio counterparts have been observed too. These events may be interpreted in terms of microlensing by a foreground galaxy.
AO 0235+16 QSO 0235+164 02 38 38.9 +16 36 59
The optical observations HJD Heliocentric Julian date d Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag Rmag R magnitude mag e_Rmag rms uncertainty on Rmag mag Imag I magnitude mag e_Imag rms uncertainty on Imag mag Obs Observer number=1 NOT: North Optical Telescope, La Palma, 2.5m, BVRI JKT: Jacobus Kapteyn telescope, La Palma, 1.0m, VR TO: Torino, 1.05m, R TU: Tuorla, 1.03m, V BO: Boltwood, 17cm, VRI PE: Perugia, 40cm, VRI --- table2.tex LaTeX version of table2 Patricia Bauer CDS 1997 Nov 21 J_A+AS_129_577.xml Surface photometry of early-type galaxies in the Hubble Deep Field J/A+AS/129/583 J/A+AS/129/583 Hubble Deep Field surface photometry Surface photometry of early-type galaxies in the Hubble Deep Field G Fasano M Filippi F Bertola Astron. Astrophys. Suppl. Ser. 129 583 1998 1998A&AS..129..583F J/AJ/112/1335 : Hubble Deep Field observations (Williams+ 1996) Galaxies, photometry Photometry, surface galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: photometry The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, <http://ecf.hq.eso.org>). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. <J/AJ/112/1335>) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.
HST/VIS
List of the 99 galaxies in the sample Name Galaxy name --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec WBD96 Simbad denomination ([WBD96] N-NNN.nnnn) --- Galaxy parameters Name Galaxy name --- mag V_606 surface brightness (ST system) mag/arcsec2 Xpos X coord. of the center pix Ypos Y coord. of the center pix Radius Radius along the major axis arcsec Eps Ellipticity = 1-b/a --- PA Position Angle from N to W deg Sin3 {3[theta] term in Fourier expansion}*10 number=1 99.00 --> data are not available 0.1 Cos3 {3[theta] term in Fourier expansion}*10 number=1 99.00 --> data are not available 0.1 Sin4 {4[theta] term in Fourier expansion}*10 number=1 99.00 --> data are not available 0.1 Cos4 {4[theta] term in Fourier expansion}*10 number=1 99.00 --> data are not available 0.1 e_Eps Estimated error of the ellipticity --- e_PA Estimated error of the position angle deg e_Sin3 Estimated error of Sin3 0.1 e_Cos3 Estimated error of Cos3 0.1 e_Sin4 Estimated error of Sin4 0.1 e_Cos4 Estimated error of Cos4 0.1 e_mag Estimated error of surface brightness mag/arcsec2 Patricia Bauer CDS 1997 Dec 11 Gianni Fasano <gfasano@leda.pd.astro.it> J_A+AS_129_583.xml Photoelectric photometry and period analysis of selected delta Scuti stars in Praesepe J/A+AS/129/9 J/A+AS/129/9 Delta Sct stars in Praesepe Photoelectric photometry and period analysis of selected delta Scuti stars in Praesepe J H Pena R Peniche M A Hobart A Rolland P Lopez de Coca M Paparo L Parrao C de la Cruz J I Olivares V Costa C Ibanoglu A Y Ertan O Tumer S Evren Z Tunca Astron. Astrophys. Suppl. Ser. 129 9 1998 1998A&AS..129....9P Clusters, open Photometry Stars, variable delta Scuti open clusters and associations: individual (Praesepe) stars: oscillations Photoelectric photometry of seven Delta Scuti stars in Praesepe was secured. Three of them were observed simultaneously at observatories located at different longitudes. Period analysis has been carried out for each star with different computing packages and the results compared to those in the literature. Their physical characteristics have been determined from the Stromgren photometry and theoretical and empirical calibrations.
KW 045 BR Cnc 08 37 40.8 +19 31 07 KW 204 BT Cnc 08 39 42.7 +19 46 43 KW 207 BU Cnc 08 39 44.7 +19 16 31 KW 284 HD 73712 08 40 20.2 +19 20 57 KW 323 BN Cnc 08 40 39.3 +19 13 43 KW 445 BX Cnc 08 42 06.6 +19 24 42
</tableLink> <tableLink xlink:href="kw204v.dat"> <title>Differential photometry of KW 204 in the V filter (in 1982) Differential photometry of KW 204 in the y filter Differential photometry of KW 207 in the y filter Differential photometry of KW 323 in the y filter Differential photometry of KW 445 in the y filter HJD Heliocentric Julian date d ymag y magnitude (V magnitude for kw204v.dat) mag Francois Ochsenbein CDS 1998 Apr 20 Jose H. Pena <jhpena@astroscu.unam.mx> J_A+AS_129_9.xml BV(RI)c monitoring of ON 231 during the great outburst in 1994-1997 J/A+AS/130/109 J/A+AS/130/109 BV BV(RI)c monitoring of ON 231 during the great outburst in 1994-1997 G Tosti M Fiorucci M Luciani M Rizzi M Villata C M Raiteri G De Francesco L Lanteri M Chiaberge A Peila M Cavallone G Sobrito M Maesano E Massaro F Montagni R Nesci G Ghisellini L O Takalo A Sillanpaa S Katajainen P Heinamaki K Nilsson T Pursimo Astron. Astrophys. Suppl. Ser. 130 109 1998 1998A&AS..130..109T J/A+AS/116/403 : VRI photometry of stars in 12 BL Lac objects (Fiorucci+, 1996) BL Lac objects Photometry, Cousins Photometry, UBVRI BL Lacertae objects: general BL Lacertae objects: individual (ON 231) We present the most continuous data base of optical multiband data ever published on the BL Lacertae object ON 231 (W Com). The data have been collected during an intensive and coordinated BV(RI)c monitoring campaign carried out in the period from March 1994 to March 1997. During our campaign, the source brightness was at the highest level ever observed. The light curve shows a complex structure, characterized by the presence of three major outbursts having the observed maxima in March 1995, February 1996, and January 1997, when ON 231 reached its historical maximum (B~=14.2). Variability on time scales from a few hours up to a month have frequently been observed and the light curve seems to be the superposition of many flares with different amplitudes and time scales. The broad-band optical spectral energy distribution is characterized by a spectral slope which correlates with the flux level. In particular, the higher is the flux the flatter is the spectrum.
ON 231 W Com OHIO N 231 12 21 27.5 +28 14 00
List of BVRI data HJd Heliocentric Julian Day d Bmag B (Johnson) magnitude and standard deviation mag e_Bmag rms uncertainty on Bmag mag Vmag V (Johnson) magnitude and standard deviation mag e_Vmag rms uncertainty on Vmag mag Rmag R (Cousins) magnitude and standard deviation mag e_Rmag rms uncertainty on Rmag mag Imag I (Cousins) magnitude and standard deviation mag e_Imag rms uncertainty on Imag mag Obs Observatory number=1 PG = Perugia RM = Roma TO = Torino TU = Tuorla ---- Patricia Bauer CDS 1997 Dec 01 Gino Tosti <TOSTI@astrpg.pg.infn.it> J_A+AS_130_109.xml Micrometer measurements of double stars from the Spanish observatories at Calar Alto and Santiago de Compostela J/A+AS/130/117 J/A+AS/130/117 Double stars micrometer measurements Micrometer measurements of double stars from the Spanish observatories at Calar Alto and Santiago de Compostela J A Docobo Astron. Astrophys. Suppl. Ser. 130 117 1998 1998A&AS..130..117D Stars, double and multiple astrometry binaries: close binaries: visual These tables report 458 micrometer observations of visual double stars made with the 152cm. telescope at Calar Alto Observatory (Almeria, Spain) and with the 35cm. telescope at Ramon Maria Aller Observatory (Santiago de Compostela, Spain).
Calar Alto observations Ramon Maria Aller observations WDS WDS (Cat. <I/237>) designation --- Name Other name (letters denote the components in the case of the multiple star system) --- ADS ADS designation --- Epoch Observation epoch yr theta Position angle deg rho Separation arcsec Nnights Number of nights on wich the star was observed --- Patricia Bauer CDS 1997 Dec 18 Jose A. Docobo <oadoco@usc.es> J_A+AS_130_117.xml UBV polarimetry of 361 A- and F-type stars in Selected Areas J/A+AS/130/133 J/A+AS/130/133 UBV polarimetry of 361 A- and F-type stars UBV polarimetry of 361 A- and F-type stars in Selected Areas A Reiz G A P Franco Astron. Astrophys. Suppl. Ser. 130 133 1998 1998A&AS..130..133R Polarization Stars, A-type Stars, distances Stars, F-type catalogs dust, extinction polarization stars: general We present simultaneous UBV linear polarization measurements for 361 A- and F-type stars with accurate colour excess and distance determination. These stars are distributed in 35 Kapteyn's Selected Areas, covering the third and fourth quadrants of the galactic plane (|b|<=30{deg}). The obtained polarization and the known colour excess are compared. An analysis of the polarization distribution as a function of the stellar distance is also performed.
UBV polarimetry of 361 stars in Selected Areas Star Star number in the Knude's catalogue (Knude, 1977A&AS...30..297K) --- HD HD (Cat. <III/135>) number --- RAh Right Ascension for the equinox 1900.0 h RAm Right Ascension for the equinox 1900.0 min RAs Right Ascension for the equinox 1900.0 s DE- Declination sign --- DEd Declination for the equinox 1900.0 deg DEm Declination for the equinox 1900.0 arcmin DEs Declination for the equinox 1900.0 arcsec GLONd Galactic longitude deg GLONm Galactic longitude arcmin GLAT- Galactic latitude (sign) --- GLATd Galactic latitude deg GLATm Galactic latitude arcmin Vmag V magnitude mag Filt Filter (U,B,V) --- Pol Polarization (P) % e_Pol Error in P % PAg Galactic position angle deg PAe Equatorial position angle deg e_PAe Error of the equatorial position angle deg E(b-y) Estimated colour excess E(b-y) (Knude, 1978A&AS...33..347K) mag Dist Estimated distance (Knude, 1978A&AS...33..347K) pc Patricia Bauer CDS 1997 Dec 04 G. Franco, <franco@sapucaia.fisica.ufmg.br> J_A+AS_130_133.xml On the use of the Hipparcos intermediate astrometric data J/A+AS/130/157 J/A+AS/130/157 Hipparcos intermediate astrometric data On the use of the Hipparcos intermediate astrometric data F van Leeuwen D W Evans Astron. Astrophys. Suppl. Ser. 130 157 1998 1998A&AS..130..157V Positional data astrometry methods: numerical Summary of the great circle statistics for FAST and NDAC reduction results, allowing the distinction of great circles according to the number of accepted single star transits.
Hipparcos
*Number of abscissa residuals per orbit, split into three types of solutions; (I) type 5; (II) types 7, 9 and X; and (III) types C, V, O and -. Orbit Sequential orbit number --- NDACIa (I) accepted, NDAC, solutions type 5 --- NDACIr (I) rejected, NDAC, --- NDACIIa (II) accepted, NDAC, solutions type 7, 9 and X --- NDACIIr (II) rejected, NDAC, --- NDACIIIa (III) accepted, NDAC, solutions type C, V, O and - --- FASTIa (I) accepted, FAST, solutions type 5 --- FASTIr (I) rejected, FAST, --- FASTIIa (II) accepted, FAST, solutions type 7, 9 and X --- FASTIIr (II) rejected, FAST, --- FASTIIIa (III) accepted, FAST, solutions type C, V, O --- Patricia Bauer CDS 1997 Nov 04 F. van Leeuwen <fvl@ast.cam.ac.uk> J_A+AS_130_157.xml Multiplicity among peculiar A stars I. The Ap stars HD 8441 and HD 137909, and the Am stars HD 43478 and HD 96391 J/A+AS/130/223 J/A+AS/130/223 Multiplicity among peculiar A stars I. Multiplicity among peculiar A stars I. The Ap stars HD 8441 and HD 137909, and the Am stars HD 43478 and HD 96391 P North J -M Carquillat N Ginestet F Carrier S Udry Astron. Astrophys. Suppl. Ser. 130 223 1998 1998A&AS..130..223N II/169 : Catalogue of observations in the Geneva photometric system Rufener F., 1988, "Catalogue of stars measured in the Geneva Observatory Photometric system", 4th Edition, Geneva Observatory (Cat. <II/169>) Binaries, spectroscopic Photometry, Geneva Radial velocities binaries: eclipsing binaries: spectroscopic catalogs stars: individual (HD 8441, HD 43478, HD 93961, HD 137909) Sun: activity Sun: flares Sun: X-rays, gamma rays Radial velocities measured with the Coravel scanner are used to determine the orbits of two Ap stars and of two Am stars. The Ap stars HD 8441 appears to be a triple system (though of SB1 type), while improved orbital elements and masses are given for the classical Ap star beta CrB. Both Am stars HD 43478 and HD 93961 are SB2 binaries, and the fundamental elements of the former can be known thanks to its eclipsing nature.
HD 8441 01 24 18.7 +43 08 32 HD 137909 15 27 50.3 +29 06 16 HD 43478 06 17 51.5 +32 30 16 HD 96391 11 08 22.0 +71 57 33
Individual CORAVEL velocities of HD 8441 Individual CORAVEL velocities of HD 137909 Individual CORAVEL velocities of HD 43478 A Individual CORAVEL velocities of HD 43478 B Individual CORAVEL velocities of HD 96391 A Individual CORAVEL velocities of HD 96391 B Date Observation date "DD/MM/YY" HJD Heliocentric Julian Day d HRV Heliocentric radial velocity km/s e_HRV individual rms error on HRV km/s Photometry of HD 43478 HJD Heliocentric Julian day d Q Photometric Q weight (Rufener 1988, Cat. <II/169>) --- [V] Magnitude in the visible mag P Photometric P weight (Rufener 1988, Cat. <II/169>) --- [U-B] Geneva [U-B] index mag [V-B] Geneva [V-B] index mag [B1-B] Geneva [B1-B] index mag [B2-B] Geneva [B2-B] index mag [V1-B] Geneva [V1-B] index mag [G-B] Geneva [G-B] index mag Patricia Bauer CDS 1998 Mar 05 Pierre North <Pierre.North@obs.unige.ch> J_A+AS_130_223.xml The WATCH Solar X-Ray Burst Catalogue J/A+AS/130/233 J/A+AS/130/233 WATCH Solar X-Ray Burst Catalogue The WATCH Solar X-Ray Burst Catalogue N Crosby N Lund N Vilmer R Sunyaev Astron. Astrophys. Suppl. Ser. 130 233 1998 1998A&AS..130..233C Sun X-ray sources catalogs Sun: activity Sun: flares Sun: X-rays, gamma rays Catalogue containing solar X-ray bursts measured by the Danish Wide Angle Telescope for Cosmic Hard X-Rays (WATCH) experiment aboard the Russian satellite GRANAT in the deca-keV energy range. Table 1 lists the periods during which solar observations with WATCH are available (WATCH ON-TIME) and where the bursts listed in the catalogue have been observed.
GRANAT
On-time catalogue DN Dump number --- StartDate Start date of dump "DD/MM/YY" Starth Start time of dump h Startm Start time of dump min Starts Start time of dump s EndDate End date of dump "DD/MM/YY" End.h End time of dump h End.m End time of dump min End.s End time of dump s WATCH solar X-ray burst catalogue DN dump number --- Date Date when burst began "DD/MM/YY" Pt Peak count rate in low-energy channel (in ct/bin) ct Tacc Accumulation time of bin (in s/bin) s Tpeak.h Peak time of burst h Tpeak.m Peak time of burst min Tpeak.s Peak time of burst s Tstart.h Start time of burst h Tstart.m Start time of burst min Tstart.s Start time of burst s n_Tstart.h N: Missing information --- Tend.h End time of burst h Tend.m End time of burst min Tend.s End time of burst s n_Tend.h N: Missing information --- B Background count rate (in ct/bin) number=1 Converted to the time accumulation of the bin. ct H Signal in high-energy channel number=2 '1' for yes, '0' for no, 'n' implies that some particle noise is observed in the high-energy channel, but not at the peak time of the burst. --- d Dead-time effect in low-energy number=3 'd' for yes, '0' for no. --- o Overflow effect in low-energy number=4 'o' for yes, '0' for no. --- AR Active region association number=5 '0' for no association. --- GOES GOES flare identification number=6 'N' for none, 'ng' implies that no GOES data exists. --- halpha H{alpha} association number=7 '1' for yes, '0' for no. --- Patricia Bauer CDS 1998 Jan 05 Norma CROSBY <ncrosby@fidji.cnrs-orleans.fr> J_A+AS_130_233.xml Four-colour photometry of eclipsing binaries. XXXIX. Light curves of the pre-main sequence triple system TY Coronae Australis J/A+AS/130/245 J/A+AS/130/245 Light curves of the PMS system TY CrA Four-colour photometry of eclipsing binaries. XXXIX. Light curves of the pre-main sequence triple system TY Coronae Australis L P R Vaz J Andersen B W Casey J V Clausen R D Mathieu I Heyer Astron. Astrophys. Suppl. Ser. 128 251 1998 1998A&AS..130..245V Binaries, eclipsing Photometry, uvby binaries: eclipsing stars: individual (TY CrA) stars: pre-main sequence Complete uvby light curves of the detached Herbig Be eclipsing binary TY Coronae Australis are presented. A total of 1787 photometric measurements in each of the four colours were obtained in 1989 and in 1992-1994. A detailed analysis of the y light curve obtained in 1992-1993 is published separately (Casey et al. 1997). The reflection nebula around the system contributes about 30% of the light in all four passbands. Here we present and discuss the non-eclipse-related photometric variability of the system. We suggest that these variations are the result of variable obscuration, possibly linked to dust shells physically associated to the system.
TY CrA 19 01 40.7 -36 52 33 HD 176423 19 01 50.3 -36 39 52
Magnitude differences TY CrA - HD 176423 in 1989, 1992, 1993 and 1994 (instrumental system) Year Year of observations yr HJD Heliocentric Julian Day d Dymag y magnitude difference mag Db-y b-y colour index difference mag Dm1 m1 Stroemgren index difference mag Dc1 c1 Stroemgren index difference mag Dbmag b magnitude difference mag Dvmag v magnitude difference mag Dumag u magnitude difference mag Patricia Bauer CDS 1997 Dec 08 Luiz Paulo R. Vaz <vaz@suya.fisica.ufmg.br> J_A+AS_130_245.xml Starbursts in barred spiral galaxies. III. Definition of a homogeneous sample of Starburst Nucleus Galaxies J/A+AS/130/285 J/A+AS/130/285 Sample of starburst nucleus galaxies Starbursts in barred spiral galaxies. III. Definition of a homogeneous sample of Starburst Nucleus Galaxies T Contini S Considere E Davoust Astron. Astrophys. Suppl. Ser. 130 285 1998 1998A&AS..130..285C VII/172 : First Byurakan Survey (FBS) (Markarian+, 1989) Contini et al., Paper I. 1995A&A...303..440C Contini et al., Paper II. 1997A&A...324...41C Active gal. nuclei Galaxies, Markarian H II regions Spectrophotometry galaxies: active galaxies: general galaxies: ISM galaxies: starburst infrared: galaxies This paper presents optical long-slit spectroscopic observations of 105 barred Markarian IRAS galaxies. These observations are used to determine the spectral type (starburst or Seyfert) of emission-line regions in the nucleus and along the bar of the galaxies, in order to define a homogeneous sample of Starburst Nucleus Galaxies (SBNGs). Our selection criteria (ultraviolet excess, far infrared emission and barred morphology) have been very efficient for selecting star-forming galaxies, since our sample of 221 emission-line regions includes 82% nuclear or extranuclear starbursts. The contamination by Seyferts is low (9%). The remaining galaxies (9%) are objects with ambiguous classification (HII or LINER). The dust content and H{alpha} luminosity increase towards the nuclei of the galaxies. No significant variation of the electron density is found between nuclear and bar HII regions. However, the mean H{alpha} luminosity and electron density in the bar are higher than in typical disk HII regions. We investigate different mechanisms for explaining the excess of nitrogen emission observed in our starburst nuclei. There is no evidence for the presence of a weak hidden active galactic nucleus in our starburst galaxies. The cause of this excess is probably a selective enrichment of nitrogen in the nuclei of the galaxies, following a succession of short and intense bursts of star formation. Our sample of SBNGs, located at a mean redshift of 0.015, has moderate H{alpha} (10^41^erg/s) and far infrared (10^10^L{sun}) luminosities. The types are distributed equally among early- and late-type giant spirals with a slight preference for Sbc/Sc types because of their barred morphology. The majority (62%) of SBNGs are isolated with no sign of gravitational interaction. In terms of distance, luminosity and level of interaction, SBNGs are intermediate between HII galaxies and luminous infrared galaxies.
Global properties of the sample Mrk Markarian (Cat. <VII/172>) number --- RAh Right ascension (1950) h DEdeg Declination (1950) deg Name Other name --- Mtype Morphological type from RC3 --- Ring Ring --- Mult Multiple system --- CType Code for morphological type (RC3) --- i Inclination angle deg HRV Heliocentric radial velocity km/s Bmag Apparent blue magnitude mag Mabs Absolute blue magnitude mag q_F12 Quality codes for the IRAS 12 micron band --- F12 Flux density at 12 micron Jy q_F25 Quality codes for the IRAS 25 micron band --- F25 Flux density at 25 micron Jy q_F60 Quality codes for the IRAS 60 micron band --- F60 Flux density at 60 micron Jy q_F100 Quality codes for the IRAS 100 micron band --- F100 Flux density at 100 micron Jy Log of spectroscopic observations Mrk Markarian (Cat. <VII/172>) number --- Date Date of observation "DD/MM/YY" Exp Exposure time min Rangel Spectral range (lower value) 0.1nm ---- --- Rangeu Spectral range (upper value) 0.1nm Width Slit width arcsec PA Position angle of the slit deg Intensity and equivalent width of emission lines Mrk Markarian (Cat. <VII/172>) number --- No Number of the emission-line region in the galaxy --- Pos Position: nuclear (1) or extranuclear (0) emission-line region --- Dist Distance between extranuclear emission-line regions and the galaxy nucleus arcsec Size Size of emission-line regions arcsec l_F(Hbeta) Limit lfag on F(Hbeta) --- F(Hbeta) H{beta} (4861) line flux number=1 Line fluxes are not corrected for reddening 10-14mW/m2 W(Hbeta) H{beta} (4861) equivalent width 0.1nm F([OIII]a) [OIII] (4959) line flux number=1 Line fluxes are not corrected for reddening 10-14mW/m2 W([OIII]a) [OIII] (4959) equivalent width 0.1nm F([OIII]b) [OIII] (5007) line flux number=1 Line fluxes are not corrected for reddening 10-14mW/m2 W([OIII]b) [OIII] (5007) equivalent width 0.1nm F([NII]a) [NII] (6548) line flux number=1 Line fluxes are not corrected for reddening 10-14mW/m2 W([NII]a) [NII] (6548) equivalent width 0.1nm F(Halpha) H{alpha} (6653) line flux number=1 Line fluxes are not corrected for reddening 10-14mW/m2 W(Halpha) H{alpha} (6653) equivalent width 0.1nm F([NII]b) [NII] (6583) line flux number=1 Line fluxes are not corrected for reddening 10-14mW/m2 W([NII]b) [NII] (6583) equivalent width 0.1nm F([SII]a) [SII] (6716) line flux number=1 Line fluxes are not corrected for reddening 10-14mW/m2 W([SII]a) [SII] (6716) equivalent width 0.1nm F([SII]b) [SII] (6731) line flux number=1 Line fluxes are not corrected for reddening 10-14mW/m2 W([SII]b) [SII] (6731) equivalent width 0.1nm Magnitude and color indices of the spectral continuum Mrk Markarian (Cat. <VII/172>) number --- No Number of the emission-line region in the galaxy --- Bmag B magnitude mag Vmag V magnitude mag Rmag R magnitude mag b-v b-v color index mag v-r v-r color index mag Derived spectrophotometric parameters Mrk Markarian (Cat. <VII/172>) number --- No Number of the emission-line region in the galaxy --- Pos nuclear (1) or extranuclear (0) emission-line region --- Dgal Distance of the galaxy (with H_0_=75km/s/Mpc) Mpc Dist Distance between extranuclear emission-line regions and the galaxy nucleus kpc Size Size of emission-line regions kpc c(Hbeta) Reddening coefficient mag NE Electronic density cm-3 log([NII]/Halpha) log([NII]6583/H{alpha}) --- log([SII]/Halpha) log([SII]6716+6731/H{alpha}) --- log([OIII]/Hbeta) log([OIII]5007/H{beta}) --- Stype Results of the spectral classification number=1 Spectral classification: - SBNG: Starburst Nucleus Galaxy - HIIG: HII Galaxy - HII: extranuclear HII region - LIN: LINER - Sey 1: Seyfert 1 - Sey 2: Seyfert 2 - SBNG,LIN ?: ambiguous classification between starburst and LINER - HII ?: uncertain classification --- I(Halpha) H{alpha} line flux corrected for reddening 10-15mW/m2 log(L(Halpha)) log of H{alpha} luminosity corrected for reddening [10-7J/s] u_I(Halpha) Uncertainty flag on I(Halpha) and log(L(Halpha)) number=2 A lower limit (:) on both the H{alpha} flux and luminosity is given if the reddening coefficient c(Hbeta) has not been determined --- Patricia Bauer CDS 1997 Dec 05 T. Contini <contini@wise1.tau.ac.il> J_A+AS_130_285.xml The ESO Slice Project (ESP) galaxy redshift survey: III. The Sample J/A+AS/130/323 J/A+AS/130/323 ESO Slice Project The ESO Slice Project (ESP) galaxy redshift survey: III. The Sample G Vettolani E Zucca R Merighi M Mignoli D Proust G Zamorani A Cappi L Guzzo D Maccagni M Ramella G M Stirpe A Blanchard V Cayatte C Collins H MacGillivray S Maurogordato R Scaramella C Balkowski G Chincarini P Felenbok Astron. Astrophys. Suppl. Ser. 130 323 1998 1998A&AS..130..323V http://boas5.bo.astro.it/~cappi/esokp.html : the databaseVettolani et al., Paper I. 1997A&A...325..954V Zucca et al., Paper II. 1997A&A...326..477Z Galaxy catalogs Radial velocities Surveys catalogs cosmology: observations galaxies: distances and redshifts galaxies: ISM radio lines: galaxies The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&A...325..954V; Zucca et al. 1997A&A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray & Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html
OPTOPUS fields Field OPTOPUS field number as in paper --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Nt No. of objects classified as galaxies in the photometric catalogue --- Nz No. of measured redshifts --- Nno No. of not observed objects --- Nf No. of failed spectra --- Ns No. of stars --- Catalogue ESP ESP galaxy number as in paper --- Field OPTOPUS field number as in paper --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec bJmag bJ magnitude --- HRVa Heliocentric radial velocity from absorption lines number=1 Codes in the velocity column: -8888 = failed radial velocity measurement -9999 = stellar spectrum (hence stars misclassified in the EDSGC) 99999 = only for the object #31954, a QSO with z=1.174 km/s e_HRVa Error on absorption line velocity km/s R R parameter value from cross-correlation --- HRVe Heliocentric radial velocity from emission lines number=1 Codes in the velocity column: -8888 = failed radial velocity measurement -9999 = stellar spectrum (hence stars misclassified in the EDSGC) 99999 = only for the object #31954, a QSO with z=1.174 km/s e_HRVe Error on emission line velocity km/s Patricia Bauer CDS 1998 Mar 26 Elena Zucca <ZUCCA@astbo1.bo.cnr.it> J_A+AS_130_323.xml Kinematics of the local universe. VII. New 21-cm line measurements of 2112 galaxies J/A+AS/130/333 J/A+AS/130/333 2112 new 21-cm line measurements Kinematics of the local universe. VII. New 21-cm line measurements of 2112 galaxies G Theureau L Bottinelli N Coudreau-Durand L Gouguenheim N Hallet M Loulergue G Paturel P Teerikorpi Astron. Astrophys. Suppl. Ser. 130 333 1998 1998A&AS..130..333T J/A+AS/102/57 : Radial Velocities of the local universe (Bottinelli+ 1993) Bottinelli et al., Paper I. 1992A&AS...93..173B Bottinelli et al., Paper II. 1993A&AS..102...57B, Cat. <J/A+AS/102/57> Di Nella et al., Paper III. 1996A&AS..118..311D Theureau et al., Paper IV. 1997A&A...319..435T Theureau et al., Paper V. 1997A&A...322..730T Theureau, Peper VI. 1998A&A...331....1T Galaxies, radio H I data Radial velocities catalogs galaxies: distances and redshifts galaxies: ISM radio lines: galaxies This catalogue contains 2112 new 21-cm neutral hydrogen line measurements carried out with the meridian transit Nancay radiotelescope. Among these data we give also 213 new radial velocities which complement those listed in three previous papers of this series. Table2.dat is the list of corrected astrophysical HI-parameters (name, coordinates, systemic heliocentric velocity, line-width at two levels, log of maximum circular velocity, HI-flux and signal to noise ratio) The folder fig5 contains the files page01.ps, page02.ps ... corresponding to Figure 5, i.e. the HI-profiles of the galaxies listed in table2.dat.
Catalogue of corrected HI-parameters PGC PGC (Cat. <VII/119>) name --- name usual name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec V20 Systemic heliocentric radial velocity km/s e_V20 rms error on V20 km/s W20 line width at 20% of the maximum km/s e_W20 rms error on W20 km/s W50 line width at 50% of the maximum km/s e_W50 rms error on W50 km/s logVm log of maximal circular velocity [km/s] e_logVm rms error on logVm [km/s] FHI calibrated HI-flux Jy.km/s e_FHI rms error on FHI Jy.km/s S/N signal to noise ratio --- Note see Note number=1 I: published in paper I (Bottinelli et al., 1992A&AS...93..173B) II: published in paper II (Bottinelli et al., 1993, Cat. <J/A+AS/102/57>) c: HI-confusion or disturbed profile a: HI-confusion but measurable parameters *: the profile does not appear in Fig.5 A: a note exists in appena.dat --- pageno Page number of figure number=2 the three numbers pageno, rowno and colno allow to locate the corresponding profile in subdirectory fig5. --- rowno Row number in page number=2 the three numbers pageno, rowno and colno allow to locate the corresponding profile in subdirectory fig5. --- colno Column number in page number=2 the three numbers pageno, rowno and colno allow to locate the corresponding profile in subdirectory fig5. --- Individual comments on Fig. 5 and table2.dat PGC PGC Name --- Name Other names --- Ntot Total number of lines for the Name --- Nline Running line number in range [1,Ntot] --- Text Text of note --- appena.tex LaTeX version of appena.dat Patricia Bauer CDS 1998 Jan 12 Gilles Theureau <Gilles.Theureau@obspm.fr> UNKNOWN UNKNOWN * 12-Jan-1998: first archived. * 23-Jul-1998: about 40 incorrect names in table2.dat were corrected at CDS, like MCG -2-13-21 which was written ESO -2-13-21 J_A+AS_130_333.xml Loose Groups of Galaxies in the Perseus-Pisces Survey J/A+AS/130/341 J/A+AS/130/341 Groups of Galaxies in PPS Loose Groups of Galaxies in the Perseus-Pisces Survey R Trasarti-Battistoni Astron. Astrophys. Suppl. Ser. 130 341 1998 1998A&AS..130..341T J/AJ/105/1251 : Pisces-Perseus supercluster. V. (Wenger+, 1993) J/AJ/105/1271 : Pisces-Perseus supercluster. VI (Giovanelli+, 1993) Galaxy catalogs Velocity dispersion catalogs galaxies: clusters: general galaxies: luminosity function, mass function large-scale structure of universe We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra & Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.
List of the values of group parameters for D_0_=0.231Mpc/h and V_0_=350km/s ID Identification of group --- Nmemb Number of members --- RAh Mean right ascension 1950 number=1 RA was originally assigned values in the interval [-1:30.0, +3:00.0], but without any value in the range [0, -1]. There was clearly an omission of the minus sign in that range, and the negative RA values were turned to standard RA values. but it is not clear whether group #54 is 23:59.9 or 00:00.1 (mail exchange with the author, July 1998) h RAm Mean right ascension 1950 number=1 RA was originally assigned values in the interval [-1:30.0, +3:00.0], but without any value in the range [0, -1]. There was clearly an omission of the minus sign in that range, and the negative RA values were turned to standard RA values. but it is not clear whether group #54 is 23:59.9 or 00:00.1 (mail exchange with the author, July 1998) min DE- Sign declination (always blank) --- DEd Mean declination 1950 deg DEm Mean declination 1950 arcmin cz Mean redshift of members km/s e_cz Velocity dispersion km/s Rp Mean pairwise separation of members number=2 Assuming h=1.0, i.e. Hubble constant H_0=100km/s/Mpc Mpc Rh Mean harmonic (virial) radius number=2 Assuming h=1.0, i.e. Hubble constant H_0=100km/s/Mpc Mpc log(L) Log of total luminosity (2) number=3 Observed luminosity, not corrected for the missed faint member galaxies [solLum] log(M) Log of virial mass number=2 Assuming h=1.0, i.e. Hubble constant H_0=100km/s/Mpc [solMass] log(M/L) Log of mass-to-light ratio (2) number=3 Observed luminosity, not corrected for the missed faint member galaxies [Sun] t(cr) Crossing time (2) number=4 Defined as (2R_p_)/(sqrt(3)e_cz_) Mpc/s/km Francois Ochsenbein, Patricia Bauer CDS 1998 Aug 20 Roberto Trasarti-Battistoni <roberto@stat.physik.uni-muenchen.de> J_A+AS_130_341.xml Faint photometric BVRc CCD sequences. The North Galactic Pole (b=85 deg) and the anticenter (l=133.2, b=-1.6 deg) J/A+AS/130/359 J/A+AS/130/359 Faint photometric BVR CCD sequences Faint photometric BVRc CCD sequences. The North Galactic Pole (b=85 deg) and the anticenter (l=133.2, b=-1.6 deg) A Spagna M G Lattanzi B J McLean G Massone B M Lasker Astron. Astrophys. Suppl. Ser. 130 359 1998 1998A&AS..130..359S Photometry, CCD Photometry, standards catalogs Galaxy: structure techniques: photometric CCD photometric standard stars in the BVRc system of Johnson and Cousins are presented for two regions of importance in studies of galactic structure and kinematics: the North galactic pole (NGP), and a second galactic plane region (GPR) toward the anticenter. Precision and accuracy are better than 0.05mag down to V=18-18.5. These data are part of the Second Guide Photometric Catalog (GSPC-II).
NGP: photometry and position of the CCD standards in fields I, II, III GPR: photometry and position of the CCD standards IdPOSS Identifier on POSS plate --- IdCCD Identifier on CCD frames number=1 The format of the CCD identifier is nnn-N, where nnn is a progressive index, while N = I,II,III identifies three different close CCD fields. --- Vmag V Johnson magnitude mag B-V B-V Johnson color index mag V-R V-R Johnson-Cousins color index mag RAh Right Ascension (J2000) h RAm Right Ascension (J2000) min RAs Right Ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec tables.tex LaTeX version of tables 3 and 4 A. Spagna Obs. Astron. Torino 1998 Jan 5 Alessandro Spagna <SPAGNA@gsc2.to.astro.it> UNKNOWN UNKNOWN CCD data were taken at Mt. Hopkins using the 1.2m telescope. The GPR (table4) was observed on October 15 1993, while the NGP fields (table3) were imaged on June 5 1994. J_A+AS_130_359.xml A radio continuum study of the Magellanic Clouds. Part VII: Discrete radio sources in the Magellanic Clouds J/A+AS/130/421 J/A+AS/130/421 Radio continuum study of the MC A radio continuum study of the Magellanic Clouds. Part VII: Discrete radio sources in the Magellanic Clouds M D Filipovic R F Haynes G L White P A Jones Astron. Astrophys. Suppl. Ser. 130 421 1998 1998A&AS..130..421F Magellanic Clouds Radio sources HII regions Magellanic Clouds radio continuum: galaxies radio continuum: ISM supernova remnants We present a study of discrete radio sources in the Magellanic Clouds (MCs) using the latest large-scale radio surveys made with the Parkes radio telescope between 1.4 and 8.55GHz. These surveys achieved higher sensitivity than previous surveys done with the Parkes telescope and so the number of discrete radio sources detected towards the MCs has increased by factor of five. Also, we have obtained improved positions, flux densities and radio spectral indices for all of these sources. A total of 483 sources towards the Large Magellanic Cloud (LMC) and 224 towards the Small Magellanic Cloud (SMC) have been detected at at least one radio frequency. Most of the MC's sources have been classified in one of three groups: SNRs, HII regions or background sources according to classification criteria established here. In total, 209 discrete radio sources in the LMC and the 37 sources in the SMC are classified here to be either HII regions or SNRs. We investigate their luminosity functions as well as the statistics of background sources behind the MCs. Also, we examine the distribution of SNRs and HII regions in the MCs.
LMC Radio Spectral Index Catalogue -Part I LMCNo Sequential number --- Source Source name --- S0.408 Flux density at 0.408 GHz Jy S0.843 Flux density at 0.843 GHz Jy S1.4old Flux density at 1.4 GHz (old) Jy S1.4 Flux density at 1.4 GHz Jy S2.3 Flux density at 2.3 GHz Jy S2.45 Flux density at 2.45 GHz Jy S2.7 Flux density at 2.7 GHz Jy S4.75 Flux density at 4.75 GHz Jy S4.85 Flux density at 4.85 GHz Jy S5.01 Flux density at 5.01 GHz Jy S8.40 Flux density at 8.40 GHz Jy S8.85 Flux density at 8.55 GHz Jy S8.80 Flux density at 8.80 GHz Jy S14.7 Flux density at 14.7 GHz Jy LMC Radio Spectral Index Catalogue -Part II LMCNo Source number --- Names Other Names --- alpha Spectral index --- e_alpha rms uncertainty on alpha --- Type Source type --- Ref References in refs.dat file --- oldAlfa Old spectral index --- Comments Comments --- SMC Radio Spectral Index Catalogue -Part I SMCNo Source number --- Source Source name --- S0.408 Flux density at 0.408 GHz Jy S0.843 Flux density at 0.843 GHz Jy S1.4old Flux density at 1.4 GHz (old) Jy S1.4 Flux density at 1.4 GHz Jy S2.45 Flux density at 2.45 GHz Jy S2.7 Flux density at 2.7 GHz Jy S4.75 Flux density at 4.75 GHz Jy S4.85 Flux density at 4.85 GHz Jy S5.01 Flux density at 5.01 GHz Jy S8.55 Flux density at 8.55 GHz Jy S8.80 Flux density at 8.80 GHz Jy SMC Radio Spectral Index Catalogue -Part II SMCNo Source number --- Names Other Names --- alpha Spectral index --- e_alpha rms uncertainty on alpha --- Type Source type --- Ref References in refs.dat file --- Alphaold Old spectral index --- Com Comments --- References for table5b.dat and table6b.dat Ref Reference number --- Aut Author name --- BibCode Simbad bibcode --- Com Comments --- Filipovic University of Western Sydney Patricia Bauer CDS 1998 Jan 05 Dr Miroslav D. Filipovic <m.filipovic@nepean.uws.edu.au> J_A+AS_130_421.xml An extensive {Delta}a-photometric survey of southern B and A type bright stars J/A+AS/130/455 J/A+AS/130/455 Delta-a photometry of southern B & A bright stars An extensive {Delta}a-photometric survey of southern B and A type bright stars N Vogt F Kerschbaum H M Maitzen M Faundez-Abans Astron. Astrophys. Suppl. Ser. 130 455 1998 1998A&AS..130..455V Stars, peculiar Stars, bright Photometry techniques: photometric stars: chemically peculiar catalogues Table 2 lists the HR and HD numbers, the run in which the observations were obtained (sometimes several observations per run and/or on several runs, a, Delta a absolute and expressed in units of the average standard deviation of normal stars from the normality line, b-y and its dereddened quantity (b-y)_0, m_1, the spectral types from the BS Catalogue and the Michigan spectral survey (where available), then a column which indicates whether the object was used for the construction of the normality line (N) or entered the group of double stars (D), and finally the peculiarity group to which the star belongs (Preston's CP1-4, {lambda} Boo, {delta} Del, emission line objects E, supergiants SG and a Barium star Ba). For a description of the {DELTA}a photometric system, see e.g. <GCPD/75>
Observational data HR HR (Cat. <V/50>) number --- HD HD (Cat. <III/135>) number --- Run Run numbers --- amag a magnitude mag Da Deviation from the normality line mag e_Da {sigma} (4.74 mmag) deviation from the normality line mmag b-y b-y colour index mag (b-y)0 Dereddenned b-y colour index mag m1 m1 colour index mag SpTypeBS Bright Star (Cat. <V/50>) spectral type --- SpTypeM Michigan Catalogues spectral type number=1 Michigan Catalogues : Cat. <III/31>, <III/51>, <III/80> and <III/133> --- Status Note on the construction number=2 Column which indicates whether the object was used for the construction of the normality line (N) or entered the group of double stars (D). --- Class Classification number=3 CP[1-4]: Preston's chemically peculiar stars Ba: Barium stars SG: supergiants E: emission line objects {delta} Del: {delta} Del type star {lambda}Boo: {lambda} Boo type star --- table2.ps PostScript version of table2 table2.tex LaTeX version of table2 Patricia Bauer CDS 1998 Feb 27 Franz Kerschbaum <kerschbaum@astro.univie.ac.at> J_A+AS_130_455.xml Stellar uvby{beta} photometry in three EUV shadow directions J/A+AS/130/477 J/A+AS/130/477 uvby{beta} photometry in 3 EUV shadow directions Stellar uvby{beta} photometry in three EUV shadow directions J Knude Astron. Astrophys. Suppl. Ser. 130 477 1998 1998A&AS..130..477K I/146 : Positions and Proper Motions - North (Roeser+, 1988) I/193 : Positions and Proper Motions - South (Bastian+ 1993) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Photometry, uvby, beta Stars, distances ISM: clouds solar neighborhood stars: distances We present the uvby{beta} data used to locate the dust and derive distances for nearby diffuse interstellar clouds in the EUV shadows lb27-31, lb165-32 and lb329+46 discovered by the Extreme Ultraviolet Explorer. The photometrically derived parallaxes of our program stars are compared to the parallaxes listed in the Hipparcos Catalog. Within the photometric distance limit of 150pc, the photometric parallaxes of 21 ``normal" stars are consistent with the Hipparcos measurements within an uncertainty of 15%. Much as expected for the Stroemgren system. Since all program stars are brighter than V=~11.5 most of them are included in the Tycho photometry. For our sample of ~200 stars we find V_by_ and V_T_ to be consistent. Few stars are common to published uvby{beta} catalogs, ~10, V and the indices compare well apart from {beta} where a zero point difference of 11mmag is noticed.
lb165-32 shadow direction lb27-31 shadow direction lb329+46 shadow direction PPM PPM (Cat. <I/146> & <I/193>) number --- HD/BD HD (Cat. <III/135>) or BD (Cat. <I/122>) number --- TYC Tycho (Cat. <I/239>) number --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec Vmag V magnitude mag b-y b-y colour index mag m1 m_1_ colour index mag c1 c_1_ colour index mag o_b-y Number of observations in ubvy --- beta {beta} colour index mag o_beta Number of observations in {beta} --- Com Comments number=1 D: unresolved duplicity in Tycho (Cat. <I/239>) data G: listed in GCVS (Cat. <II/172>) R: weak indication of duplicity combined with indication of variability in Tycho (Cat. <I/239>) data S: suspected duplicity from Tycho (Cat. <I/239>) data U: apparent variability W: suspected variability Stars without PPM, HD/DM or Tycho identification are listed by a working number in this column --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Mar 20 J. Knude <indus@astro.ku.dk> UNKNOWN UNKNOWN Some errors where corrected on 22-Oct-1998 Table1.dat : PPM 93496 misprint for PPM 92496 Table2.dat : HD 198182 misprint for HD 198172 HD 238053 misprint for HD 198825 Table3.dat : PPM 282222 misprint for PPM 228222 J_A+AS_130_477.xml Calcium triplet synthesis J/A+AS/130/513 J/A+AS/130/513 Calcium triplet synthesis Calcium triplet synthesis M L Garcia-Vargas M Molla A Bressan Astron. Astrophys. Suppl. Ser. 130 513 1998 1998A&AS..130..513G Equivalent widths Models, evolutionary galaxies: elliptical and lenticular, cD galaxies: starburst galaxies: stellar content We present theoretical equivalent widths for the sum of the two strongest lines of the calcium triplet, CaT index, in the near-IR ({lambda}{lambda} 8542, 8662{AA}), using evolutionary synthesis techniques and the most recent models and observational data for this feature in individual stars. We compute the CaT index for Single Stellar Populations (instantaneous burst, standard Salpeter-type IMF at four different metallicities, Z=0.004, 0.008, 0.02 (solar) and 0.05, and ranging in age from very young bursts of star formation (few Myr) to old stellar populations, up to 17Gyr, representative of galactic globular clusters, elliptical galaxies and bulges of spirals. The interpretation of the observed equivalent widths of CaT in different stellar systems is discussed. Composite-population models are also computed as a tool to interpret the CaT detections in star-forming regions, in order to disentangle between the component due to Red Supergiant stars, RSG, and the underlying, older, population. CaT is found to be an excellent metallicity-indicator for populations older than 1 Gyr, practically independent of the age. We discuss its application to remove the age-metallicity degeneracy, characteristic of all studies of galaxy evolution based on the usual integrated indices (both broad band colors and narrow band indices). The application of the models computed here to the analysis of a sample of elliptical galaxies will be discussed in a forthcoming paper Gorgas et al. 1997).
*Synthetic Luminosities logAge Cluster age [yr] Z Metalicity value value relative to the Sun Sun LUV Luminosity in the UV (at 2000{AA}) Sun Lopt Luminosity in the optical (at 4850{AA}), representative of the continuum near H{beta} Sun LIR Luminosity in the infrared (at 2.17{mu}m, near Br_{gamma}_) Sun *Synthetic Calcium Triplet Equivalent Widths, according to Jorgensen et al. (1992A&A...254..258J) theoretical calibrations (II). Synthetic Calcium Triplet Equivalent Widths, according to Diaz et al. (1989MNRAS.239..325D, DTT89) empirical calibrations (I). logAge Single Stellar Population (SSP) age [yr] Z Metallicity value relative to the Sun Sun Lcont Continuum luminosity from the SSP number=1 Nebular emission not included, taking an average value in the DTT89's spectral band-pass Sun LCaII Luminosity absorbed in the Ca II lines at 8542 and 8662{AA} by the stars of the SSP Sun EW(CaT) Equivalent width of CaT number=2 Computed as the ratio between LCAII and the total continuum luminosity, in which both the stellar and the nebular contribution are taken into account (the lines at 8542, 8662 {AA}) 0.1nm Two-Populations composite models according to Jorgensen et al. (1992A&A...254..258J) calibrations. Three-Populations composite models according to Jorgensen et al. (1992A&A...254..258J) calibrations. Two-Populations composite models according to Diaz et al. (1989MNRAS.239..325D) calibrations. Three-Populations composite models according to Diaz et al. (1989MNRAS.239..325D) calibrations. Prop Proportion of the populations considered number=1 P is the ratio of the continuum luminosity at 6500{AA} (close to H{alpha}) of the young and intermediate population (when present) to the total light. As an example, P=0.10 indicates a model in which the population characteristic of the region (young or young+intermediate) is contributing 10% to the total light in the continuum at H{alpha}. If P is not given, a single population, or a combination of two coexisting young populations contributing 50% in mass each, have been considered. --- Age1 Age of the first population number=2 Age1=2.5 + Age2=10000 correspond to a model in which a young burst of 2.5Myr is combined with an old population of 10Gyr. Myr n_Age1 + when more than one population --- Age2 Age of the second population Myr n_Age2 + when more than two populations --- Age3 Age of the third population Myr Z Metallicity value relative to the Sun Sun EW(CaT) Equivalent width of CaT in absorption 0.1nm EW(Hb) Equivalent width of H{beta} in emission number=3 If this value is missing then the adopted population(s) is (are) too old to produce ionizing photons 0.1nm tables.tex LaTeX version of the tables tables.ps PostScript version of tables Patricia Bauer CDS 1998 Jun 18 Maria Luisa Garcia Vargas <mgarcia@ll.iac.es> J_A+AS_130_513.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest. XIX: Na X spectral lines J/A+AS/130/539 J/A+AS/130/539 Stark broadening of Na X Stark broadening of spectral lines of multicharged ions of astrophysical interest. XIX: Na X spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 130 539 1998 1998A&AS..130..539D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines J/A+AS/127/295 : Stark broadening of Kr II lines J/A+AS/127/543 : Stark broadening of S V lines J/A+AS/128/203 : Stark broadening of Mn, Ga & Ge multiplets J/A+AS/128/359 : Stark broadening of Ca IX and Ca X lines J/A+AS/129/155 : Stark broadening of Si XI and Si XIII lines Atomic physics atomic data line: profiles Using a semiclassical perturbation approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 57 Na X multiplets for perturber densities 10^17^-10^24^cm^-3^ and temperatures T=200000-5000000K. For lower perturber densities, the Stark broadening parameters are proportional to the perturber density.
Stark broadening parameters due to e-, p- and He III-impacts for Na X N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We (4) --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de (4) --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp (4) --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp (4) --- dp shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ (4) --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ (4) --- dHe++ shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1998 Jan 06 Dr Milan Dimitrijevic <mdimitrijevic@aob.bg.ac.yu> J_A+AS_130_539.xml Calculated oscillator strengths of singly ionized Cobalt J/A+AS/130/541 J/A+AS/130/541 Co II oscillator strengths Calculated oscillator strengths of singly ionized Cobalt A J J Raassen J C Pickering P H M Uylings Astron. Astrophys. Suppl. Ser. 130 541 1998 1998A&AS..130..541R Atomic physics atomic data ISM: abundances stars: chemically peculiar supernovae: general In table 2 the log(gf) values for the 3d^8^+3d^7^ 4s-->3d^7^ 4p electric dipole (E1) transitions are given. This system is selected by cutting off energy values larger than 120,000cm^-1^ of both the even and the odd system in the final printing procedure; only log(gf) values larger than -3 are included. The first column of this table shows the wavelength obtained from the energy differences between the experimental level values. Wavelengths below 2000 Angstrom are given as vacuum wavelengths and above 2000 Angstrom as air wavelengths. The second column gives the log(gf) values followed by the J-value, energy value and the name of the lower (even) level. The first character of the level name designates the configuration number: for the even levels '1' refers to 3d^8^ and '2' to 3d^7^ 4s; for the odd levels '1' refers to 3d^7^ 4p. An '*' after the energy value indicates that the level is known, in which case the experimental level value is given. When unknown, the calculated energy value is given and used to approximate the wavelength. The A-values for the forbidden lines given in table 7 are restricted to the magnetic dipole (M1) and electric quadrupole (E2) transitions within the 3d^8^+3d^7^ 4s configurations, from levels with an energy of less than 50,000 cm^-1^ above the ground and with A-values larger than 10^-3^s^-1^. The level with the lower J-value is given first in the designation of the transition. The remaining columns are similar to the corresponding ones in table 2. The first character of the level name designates the configuration number: for the even levels '1' refers to 3d^8 and '2' to 3d^7 4s. An '*' after the energy value indicates that the level is known, in which case the experimental level value is given. When unknown, the calculated energy value is given and used to approximate the wavelength.
log(gf) values for the 3d^8^+3d^7^ 4s-->3d^7^ 4p electric dipole (E1) transitions Lambda Wavelength 0.1nm loggf log(gf) value --- Jf J-value final state --- Ef Energy value final state cm-1 n_Ef Indication known/unknown --- Lf Leading term final state --- Ji J-value initial state --- Ei Energy value initial state cm-1 n_Ei Indication known/unknown --- Li Leading term initial state --- A-values for the forbidden lines lambda Wavelength 0.1nm A(M1) A-value (M1) s-1 A(E2) A-value (E2) s-1 Jf J-value final state --- Ef Energy value final state cm-1 n_Ef Indication known/unknown --- Lf Leading term final state --- Ji J-value initial state --- Ei Energy value initial state cm-1 n_Ei Indication known/unknown --- Li Leading term initial state --- Patricia Bauer CDS 1998 Jan 23 P. Uylings <uylings@phys.uva.nl> J_A+AS_130_541.xml A standard stellar library for evolutionary synthesis: II. The M dwarf extension J/A+AS/130/65 J/A+AS/130/65 A standard stellar library. II. A standard stellar library for evolutionary synthesis: II. The M dwarf extension T Lejeune F Cuisinier R Buser Astron. Astrophys. Suppl. Ser. 130 65 1998 1998A&AS..130...65L VI/39 : Model Atmospheres (Kurucz, 1979) VI/78 : Theoretical Stellar Flux Spectra for F- to K-type Stars (Buser+ 1992) J/A+AS/105/311 : M giants spectra and photometry (Fluks+, 1994) J/A+AS/125/229 : A standard stellar library (Lejeune+ 1997) Atlases Models, evolutionary Photometry, UBVRIJKLMNH Stars, late-type stars: fundamental parameters stars: late-type A standard library of theoretical stellar spectra intended for multiple synthetic photometry applications including spectral evolutionary synthesis is presented. The grid includes M dwarf model spectra, hence complementing the first library version established in Paper I (Lejeune et al., 1997, Cat. <J/A+AS/125/229>). It covers the following wide ranges of fundamental parameters: Teff: 50,000 to 2000K, logg: 5.5 to -1.02, and [Fe/H]: +1.0 to -5.0. A correction procedure is also applied to the theoretical spectra in order to provide color-calibrated flux distributions over a large domain of effective temperatures. Empirical Teff-color calibrations are constructed between 11500K and 2000K, and semi-empirical calibrations for non-solar abundances ([Fe/H]=-3.5 to +1.0) are established. Model colors and bolometric corrections for both the original and the corrected spectra, synthesized in the UBV(RI)c(JHKLL'M) system, are given for the full range of stellar parameters. Synthetic colors: ---------------- Synthetic UBV(RI)c(JHKLM) colors have been computed from both the original and the corrected model flux distributions presented in Paper I (1997A&AS..125..229L; see catalog <J/A+AS/125/229>), as the files lcb98ori.dat and lcb98cor.dat respectively; the results are also presented in individual files lcb98xxx.ori and lcb98xxx.cor, where xxx designates the metallicity (ex: 'm15' --> [Fe/H]=-1.5). For each file, we give synthetic colors computed from energy-weighted and photon-weighted stellar fluxes. Semi-empirical calibrations: --------------------------- Empirical ([Fe/H]=0.0) and semi-empirical (-3.5<=[Fe/H]<=+1.0) Teff-colors (UBVRIJHKLM) calibrations are given in Tables 1 to 10.
[Fe/H]=0.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-3.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-3.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-2.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-2.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-1.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-1.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-0.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=+0.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=+1.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections Type d: dwarf; g: giant --- Teff Effective temperature K U-B (U-B) colour mag B-V (B-V) colour mag V-I (V-I) colour mag V-K (V-K) colour mag R-I (R-I) colour mag J-H (J-H) colour mag H-K (H-K) colour mag J-K (J-K) colour mag K-L (K-L) colour mag BCVmag Bolometric correction in V (energy-weighted) mag logg Surface gravity --- [Fe/H] Metallicity [Sun] Synthetic colors from corrected SEDS at [Fe/H] = -0.1 Synthetic colors from corrected SEDS at [Fe/H] = -0.2 Synthetic colors from corrected SEDS at [Fe/H] = -0.3 Synthetic colors from corrected SEDS at [Fe/H] = -0.5 Synthetic colors from corrected SEDS at [Fe/H] = -1.0 Synthetic colors from corrected SEDS at [Fe/H] = -1.5 Synthetic colors from corrected SEDS at [Fe/H] = -2.0 Synthetic colors from corrected SEDS at [Fe/H] = -2.5 Synthetic colors from corrected SEDS at [Fe/H] = -3.0 Synthetic colors from corrected SEDS at [Fe/H] = -3.5 </tableLink> <tableLink xlink:href="lcb98m45.cor"> <title>Synthetic colors from corrected SEDS at [Fe/H] = -4.5 Synthetic colors from corrected SEDS at [Fe/H] = -5.0 Synthetic colors from corrected SEDS at [Fe/H] = 0.0 Synthetic colors from corrected SEDS at [Fe/H] = 0.1 Synthetic colors from corrected SEDS at [Fe/H] = 0.2 Synthetic colors from corrected SEDS at [Fe/H] = 0.3 Synthetic colors from corrected SEDS at [Fe/H] = 0.5 Synthetic colors from corrected SEDS at [Fe/H] = 1.0 Synthetic colors from original SEDS at [Fe/H] = -0.1 Synthetic colors from original SEDS at [Fe/H] = -0.2 Synthetic colors from original SEDS at [Fe/H] = -0.3 Synthetic colors from original SEDS at [Fe/H] = -0.5 Synthetic colors from original SEDS at [Fe/H] = -1.0 Synthetic colors from original SEDS at [Fe/H] = -1.5 Synthetic colors from original SEDS at [Fe/H] = -2.0 Synthetic colors from original SEDS at [Fe/H] = -2.5 Synthetic colors from original SEDS at [Fe/H] = -3.0 Synthetic colors from original SEDS at [Fe/H] = -3.5 Synthetic colors from original SEDS at [Fe/H] = -4.0 Synthetic colors from original SEDS at [Fe/H] = -4.5 Synthetic colors from original SEDS at [Fe/H] = -5.0 Synthetic colors from original SEDS at [Fe/H] = 0.0 Synthetic colors from original SEDS at [Fe/H] = 0.1 Synthetic colors from original SEDS at [Fe/H] = 0.2 Synthetic colors from original SEDS at [Fe/H] = 0.3 Synthetic colors from original SEDS at [Fe/H] = 0.5 Synthetic colors from original SEDS at [Fe/H] = 1.0 [Fe/H]=0.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-3.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-3.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-2.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-2.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-1.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-1.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=-0.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=+0.5 empirical UBVRIJHKLM colors and theoretical bolometric corrections [Fe/H]=+1.0 empirical UBVRIJHKLM colors and theoretical bolometric corrections All empirical UBVRIJHKLM colors and theoretical bolometric corrections (tables 1-10) All files lcb98*.ori: Synthetic colors from original Stellar Energy Distributions (SEDS) All files lcb98*.cor: Synthetic colors from corrected Stellar Energy Distributions (SEDS) Teff Effective temperature K logg Surface gravity --- [Fe/H] Metallicity [Sun] BOL Bolometric magnitude mag BCVmag Bolometric correction in V (energy-weighted) mag U-B (U-B) colour (energy-weighted) mag B-V (B-V) colour (energy-weighted) mag V-R (V-R) colour (energy-weighted) mag V-I (V-I) colour (energy-weighted) mag V-K (V-K) colour (energy-weighted) mag R-I (R-I) colour (energy-weighted) mag I-K (I-K) colour (energy-weighted) mag J-H (J-H) colour (energy-weighted) mag H-K (H-K) colour (energy-weighted) mag K-L (K-L) colour (energy-weighted) mag J-K (J-K) colour (energy-weighted) mag J-L (J-L) colour (energy-weighted) mag J-L' (J-L')colour (energy-weighted) mag K-M (K-M) colour (energy-weighted) mag BCVmagp Bolometric correction in V (photon-weighted) mag U-Bp (U-B) colour (photon-weighted) mag B-Vp (B-V) colour (photon-weighted) mag V-Rp (V-R) colour (photon-weighted) mag V-Ip (V-I) colour (photon-weighted) mag V-Kp (V-K) colour (photon-weighted) mag R-Ip (R-I) colour (photon-weighted) mag I-Kp (I-K) colour (photon-weighted) mag J-Hp (J-H) colour (photon-weighted) mag H-Kp (H-K) colour (photon-weighted) mag K-Lp (K-L) colour (photon-weighted) mag J-Kp (J-K) colour (photon-weighted) mag J-Lp (J-L) colour (photon-weighted) mag J-L'p (J-L')colour (photon-weighted) mag K-Mp (K-M) colour (photon-weighted) mag Patricia Bauer CDS 1998 Jun 18 Thibault Lejeune <lejeune@astro.unibas.ch> J_A+AS_130_65.xml Astrometry of Satellites I to V of Uranus J/A+AS/130/77 J/A+AS/130/77 Astrometry of Satellites of Uranus Astrometry of Satellites I to V of Uranus D H P Jones D B Taylor I P Williams Astron. Astrophys. Suppl. Ser. 130 77 1998 1998A&AS..130...77J Planets Positional data astrometry planets and satellites: individual (satellites of Uranus) Table7 contains standard Co-ordinates (J2000.0) in arcseconds relative to the reference satellite. The numbers of the satellites 1-5 correspond to the conventional designation of the satellites I-V.
Differential Positions of Satellites I to V of Uranus MJD Modified Julian Date (Topocentric UTC, JD-2400000) d NO Number of Satellites Observed --- NR Number of Reference Satellite --- SG Seeing (FWHM) arcsec NS1 Number of first satellite measured --- Xi1 Xi of first satellite J2000.0 arcsec Eta1 Eta of first satellite J2000.0 arcsec NS2 Number of second satellite measured --- Xi2 Xi of second satellite J2000.0 arcsec Eta2 Eta of second satellite J2000.0 arcsec NS3 Number of third satellite measured --- Xi3 Xi of third satellite J2000.0 arcsec Eta3 Eta of third satellite J2000.0 arcsec NS4 Number of fourth satellite measured --- Xi4 Xi of fourth satellite J2000.0 arcsec Eta4 Eta of fourth satellite J2000.0 arcsec Patricia Bauer CDS 1997 Nov 26 Derek Jones <dhpj@ast.cam.ac.uk> J_A+AS_130_77.xml Southern and equatorial irregular variables. II. Optical spectroscopy J/A+AS/131/119 J/A+AS/131/119 Spectroscopy of irregular variables Southern and equatorial irregular variables. II. Optical spectroscopy D Cieslinski J E Steiner F J Jablonski Astron. Astrophys. Suppl. Ser. 131 119 1998 1998A&AS..131..119C J/A+AS/124/55 : Photometry of irregular variables (Cieslinski+ 1997) Spectroscopy Stars, variable novae, cataclysmic variables stars: emission-line, Be stars: variables: general The results of optical spectroscopy of 169 southern and equatorial objects previously known as irregular variables are presented. The targets were selected via photoelectric UBV photometry among objects classified as L, L:, I, I:, IS and IS: in the General Catalogue of Variable Stars and New Catalogue of Suspected Variable Stars. Among these objects we have identified 8 cataclysmic variables, 8 symbiotic stars and stars that belong to a variety of other classes.
Spectroscopic data Name Star name --- JD Julian date of the beginning of the observation d ExpTime Exposure time s <B-V> Mean B-V colour index mag Origin Site of the observation --- Rem Remarks number=1 * : Site of the observation: CTIO - Cerro Tololo Interamerican Observatory, Chile and LNA - Laboratorio Nacional de Astrofisica/CNPq, Brazil 1 : Classified as Mira variable in Cieslinski et al. (1997IBVS.4528....1C) 2 : Average spectra 3 : V934 Aql - north component 4 : V934 Aql - south component 5 : FX Ara - north component 6 : FX Ara - east component 7 : FX Ara - south component 8 : V817 Ara - north component 9 : V817 Ara - south component 10 : Spectra are also shown in Cieslinski et al. (1994A&AS..106..243C) 11 : Quoted as suspected of cataclysmic variable in Vogt & Bateson (1982A&AS...48..383V) and Downes & Shara (1993, Cat. <V/79>) 12 : Quoted as UX UMa type in Sion & Guinan (1983IAUCo..72...41S), Downes & Shara (1993, Cat. <V/79>) and Zwitter & Munari (1994, A&AS..107..503Z) 13 : Quoted as suspected of cataclysmic variable of Z Cam type in the GCVS4 (Cat. <II/139>) 14 : Quoted as suspected of cataclysmic variable of U Gem type in the GCVS4 (Cat. <II/139>) and in Downes et al. (1997, Cat. <V/94>) 15 : Quoted as variable of the R CrB type in the GCVS4 (Cat. <II/139>) 16 : HN Sct - north component 17 : HN Sct - south component 18 : Classified as symbiotic stars in Cieslinski et al. (1997A&AS..124...57C) 19 : NSV 10348 - south component 20 : NSV 10348 - north component --- SpType Spectral type and comments about the spectrum --- Patricia Bauer CDS 1998 May 20 Deonisio Cieslinski <deo@das.inpe.br> J_A+AS_131_119.xml Flux density monitoring of radio sources with detected or supposed gamma-ray emission J/A+AS/131/11 J/A+AS/131/11 Radio sources related to gamma-ray emission Flux density monitoring of radio sources with detected or supposed gamma-ray emission W Reich P Reich M Pohl R Kothes R Schlickeiser Astron. Astrophys. Suppl. Ser. 131 11 1998 1998A&AS..131...11R Gamma rays Radio sources BL Lacertae objects: general extragalactic radio sources gamma rays quasars: general variability Table 2 lists the individual flux density measurements for 47 radio sources as observed with the Effelsberg 100-m telescope.
Radio source positions Name Radio source designation --- Other Other name --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Flux densities for 47 sources Name Radio source designation --- Year Fractional year (1900+) yr Date Date "DD/MM/YY" Freq Frequency MHz FMHz Peak flux density Jy e_FMHz Error of peak flux density Jy Patricia Bauer CDS 1998 Mar 05 Wolfgang Reich <wreich@mpifr-bonn.mpg.de> J_A+AS_131_11.xml Einstein A-Coefficients for rotational transitions in the ground vibrational state of ^28^SiC_2_, ^29^SiC_2_ and ^30^SiC_2_ J/A+AS/131/137 J/A+AS/131/137 Einstein A-Coefficients in SiC2 transitions Einstein A-Coefficients for rotational transitions in the ground vibrational state of ^28^SiC_2_, ^29^SiC_2_ and ^30^SiC_2_ S R Chandra Astron. Astrophys. Suppl. Ser. 131 137 1998 1998A&AS..131..137C J/A+AS/114/175 : Einstein A-coefficients in CS transitions (Chandra+ 1995) J/A+AS/117/557 : Einstein coefficients for CO transitions (Chandra+ 1996) Atomic physics ISM: molecules molecular data radio lines: stars stars: individual (IRC+10 216) Einstein A-coefficients for the electric dipole transitions in Silicon Dicarbide molecule and its isotopomers between rotational levels of the ground vibrational state up to 51cm^-1^ are calculated. These coefficients are used for computing radiative life times of the levels. The A-coefficients are one of the important input parameters for the radiative transfer calculations.
Einstein A-coefficients for the rotational transitions in the ground vibrational state of ^28^SiC_2_ Einstein A-coefficients for the rotational transitions in the ground vibrational state of ^29^SiC_2_ Einstein A-coefficients for the rotational transitions in the ground vibrational state of ^30^SiC_2_ J' Rotational quantum number J' --- K'a Sub-quantum number K'_a_ number=1 K_a_, K_c_: odd, even <--> odd, odd (para-transition) even, odd <--> even, even (ortho-transition) K_a_ and K_c_ are sub-quantum numbers and each of them can assume the values ranging from 0 to J. --- K'c Sub-quantum number K'_c_ number=1 K_a_, K_c_: odd, even <--> odd, odd (para-transition) even, odd <--> even, even (ortho-transition) K_a_ and K_c_ are sub-quantum numbers and each of them can assume the values ranging from 0 to J. --- J Rotational quantum number J --- Ka Sub-quantum number K_a_ number=1 K_a_, K_c_: odd, even <--> odd, odd (para-transition) even, odd <--> even, even (ortho-transition) K_a_ and K_c_ are sub-quantum numbers and each of them can assume the values ranging from 0 to J. --- Kc Sub-quantum number K_c_ number=1 K_a_, K_c_: odd, even <--> odd, odd (para-transition) even, odd <--> even, even (ortho-transition) K_a_ and K_c_ are sub-quantum numbers and each of them can assume the values ranging from 0 to J. --- A Einstein A coefficient s-1 Energies and radiative lifetimes for the rotational levels in the ground vibrational state 28^SiC_2_, ^29^SiC_2_ and ^30^SiC_2_ J' Rotational quantum number J' --- K'a Sub-quantum number K'_a_ number=1 K_a_, K_c_: odd, even <--> odd, odd (para-transition) even, odd <--> even, even (ortho-transition) K_a_ and K_c_ are sub-quantum numbers and each of them can assume the values ranging from 0 to J. --- K'c Sub-quantum number K'_c_ number=1 K_a_, K_c_: odd, even <--> odd, odd (para-transition) even, odd <--> even, even (ortho-transition) K_a_ and K_c_ are sub-quantum numbers and each of them can assume the values ranging from 0 to J. --- E(28SiC2) Energy for ^28^SiC_2_ cm-1 T(28SiC2) Radiative lifetime for ^28^SiC_2_ s E(29SiC2 Energy for ^29^SiC_2_) cm-1 T(29SiC2) Radiative lifetime for ^29^SiC_2_ s E(30SiC2 Energy for ^30^SiC_2_) cm-1 T(30SiC2) Radiative lifetime for ^30^SiC_2_ s Patricia Bauer CDS 1998 Feb 13 Suresh Chandra <sch@iucaa.iucaa.ernet.in> J_A+AS_131_137.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest. XX: O VII and Mg XI spectral lines J/A+AS/131/141 J/A+AS/131/141 Stark broadening of O VII and Mg XI Stark broadening of spectral lines of multicharged ions of astrophysical interest. XX: O VII and Mg XI spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 131 141 1998 1998A&AS..131..141D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines J/A+AS/127/295 : Stark broadening of Kr II lines J/A+AS/127/543 : Stark broadening of S V lines J/A+AS/127/543 : Stark broadening of Ca IX and Ca X lines J/A+AS/128/203 : Stark broadening of Mn, Ga & Ge multiplets J/A+AS/129/155 : Stark broadening of Si XI and Si XIII lines J/A+AS/130/539 : Stark broadening of Na X J/A+AS/131/143 : Stark broadening of Sc X, Sc XI, Ti XI and Ti XII Atomic physics atomic data line: profiles plasmas Using a semiclassical perturbation approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 14 O VII and 18 Mg XI multiplets. For O VII, perturber densities are 10^17^-10^23^cm^-3^ and temperatures T=100000-2000000K. For Mg XI, perturber densities are 10^18^-10^24^cm^-3^ and temperatures T=500000-5000000K. For lower perturber densities, the Stark broadening parameters are proportional to the perturber density.
Stark broadening parameters due to e-, p- and He III-impacts for O VII Stark broadening parameters due to e-, p- and He III-impacts for Mg XI N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- de Shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dp Shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dHe++ Shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1998 Feb 05 Dr Milan Dimitrijevic <mdimitrijevic@aob.aob.bg.ac.yu> J_A+AS_131_141.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest. XXI: Sc X, Sc XI, Ti XI and Ti XII spectral lines J/A+AS/131/143 J/A+AS/131/143 Stark broadening of Sc X & XI, Ti XI & XII Stark broadening of spectral lines of multicharged ions of astrophysical interest. XXI: Sc X, Sc XI, Ti XI and Ti XII spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 131 143 1998 1998A&AS..131..143D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines J/A+AS/127/295 : Stark broadening of Kr II lines J/A+AS/127/543 : Stark broadening of S V lines J/A+AS/128/203 : Stark broadening of Mn II,Mn III, Ga III, Ge III & Ge IV J/A+AS/128/359 : Stark broadening of Ca IX and Ca X lines J/A+AS/129/155 : Stark broadening of Si XI and Si XIII lines J/A+AS/130/539 : Stark broadening of Na X J/A+AS/131/141 : Stark broadening of O VII and Mg XI Atomic physics atomic data line: profiles plasmas By using the semiclassical-perturbation formalism, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 Sc X, 10 Sc XI, 4 Ti XI and 27 Ti XII multiplets, significant for analysis, investigation and modeling of different plasmas in solar and stellar physics, physics and technology. The results are presented as a function of temperature and perturber density.
Stark broadening parameters due to e-, p- and He III-impacts for Sc X Stark broadening parameters due to e-, p- and He III-impacts for Sc XI Stark broadening parameters due to e-, p- and He III-impacts for Ti XI Stark broadening parameters due to e-, p- and He III-impacts for Ti XII N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- de Shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dp Shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ Validity of impact approximation number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V = collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dHe++ Shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1998 Feb 17 Dr Milan Dimitrijevic mdimitrijevic@aob.bg.ac.yu J_A+AS_131_143.xml Atomic data from the IRON Project. XXXI. Electron impact excitation of optically allowed and intercombination electric dipole transitions in FeXII J/A+AS/131/153 J/A+AS/131/153 IRON Project XXXI. Fe XII electron excitation Atomic data from the IRON Project. XXXI. Electron impact excitation of optically allowed and intercombination electric dipole transitions in FeXII A M Binello H E Mason P J Storey Astron. Astrophys. Suppl. Ser. 131 153 1998 1998A&AS..131..153B J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions J/A+AS/123/159 : IRON Project XXII. C and O radiative rates J/A+AS/123/575 : IRON Project XXIII. Fe XXII excitation rate coefficients J/A+AS/126/373 : IRON Project XXVII. Fe IV collision strengths 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths 1997A&AS..122..167B : IRON Project XX. Fe I oscillator strengths 1997A&AS..122..177P : IRON Project XXI. Fe I fine-structure transition 1997A&AS..126..105B : IRON Project XXIV. Fe XXIV electron excitation 1998A&AS..127..545B : IRON Project XXV. Fe XII electron excitation 1997A&AS..126..365B : IRON Project XXVI. Fe IV oscillator strengths 1998A&AS..129..161B : IRON Project XXVIII. F-like ions fine-structure trans. Atomic physics atomic data atomic processes Sun: UV radiation The following tables list energy levels and electron excitation data for the lowest 41 levels of Fe XII (configurations 3s^2^ 3p^3, 3s 3p^4^ and 3s^2 ^3p^2^ 3d). The table numbers correspond to the numbering given in the paper
Energy levels for the lowest three configurations in Fe XII Conf Configuration --- Level Intermediate coupling level --- EObs Observed energy cm-1 ETh Theoretical energy cm-1 Partial R-matrix and Coulomb-Bethe collision strengths for l=14,15,16 at E=100Ry Trans Transition --- R14 Partial R-matrix collision strength for l=14 --- C14 Partial C-Be collision strength for l=14 --- R15 Partial R-matrix collision strength for l=15 --- C15 Partial C-Be collision strength for l=15 --- R16 Partial R-matrix collision strength for l=16 --- C16 Partial C-Be collision strength for l=16 --- Collision strengths for all electric dipole fine-structure transitions between the ground 3s^2^ 3p^3^ and the first excited 3s 3p^4^ configurations in FeXII Trans Transition --- OP6 Collision strength at 6.6 Ry --- OT6 Collision strength by TH88 at 6.6 Ry number=1 TH88: Tayal S.S. & Henry R.J.W., 1988ApJ...329.1023T F77: Flower D.R., 1977A&A....54..163F --- OF6 Collision strength by F77 at 6.6 Ry number=1 TH88: Tayal S.S. & Henry R.J.W., 1988ApJ...329.1023T F77: Flower D.R., 1977A&A....54..163F --- OP3 Collision strength at 30 Ry --- OT3 Collision strength by TH88 at 30 Ry number=1 TH88: Tayal S.S. & Henry R.J.W., 1988ApJ...329.1023T F77: Flower D.R., 1977A&A....54..163F --- Collision strengths for all electric dipole fine-structure transitions between the ground 3s^2^ 3p^3^ and the second excited 3s^2^ 3p^2^ 3d configurations in FeXII Trans Transition --- OP Collision strength at 6.6 Ry --- OF Collision strength by F77 at 6.6 Ry number=1 F77: Flower D.R., 1977A&A....54..163F --- Effective collision strengths for all electric dipole fine-structure transitions between the ground 3s^2^ 3p^3^ and the first excited 3s 3p^4^ configurations in FeXII. Temperatures in the range 4x10^5K-3x10^6K Effective collision strengths for all electric dipole fine-structure transitions between the ground 3s^2 3p^3 and the second excited 3s^2 3p^2 3d configurations in FeXII. Temperatures in the range 4x10^5K-3x10^6K Trans Transition --- U04 Effective collision strength at 4x10^5^K --- U06 Effective collision strength at 6x10^5^K --- U08 Effective collision strength at 8x10^5^K --- U10 Effective collision strength at 10^6^K --- U12 Effective collision strength at 1.2x10^6^K --- U14 Effective collision strength at 1.4x10^6^K --- U16 Effective collision strength at 1.6x10^6^K --- U18 Effective collision strength at 1.8x10^6^K --- U20 Effective collision strength at 2x10^6^K --- U25 Effective collision strength at 2.5x10^6^K --- U30 Effective collision strength at 3x10^6^K --- Effective collision strengths for all electric dipole fine-structure transitions between the ground 3s^2^ 3p^3^ and the first excited 3s 3p^4^ configurations in FeXII. Temperatures in the range 4x10^6K-10^7K Effective collision strengths for all electric dipole fine-structure transitions between the ground 3s^2 3p^3 and the second excited 3s^2 3p^2 3d configurations in FeXII. Temperatures in the range 4x10^6K-10^7K Trans Transition --- U04 Effective collision strength at 4x10^6 K --- U05 Effective collision strength at 5x10^6 K --- U06 Effective collision strength at 6x10^6 K --- U07 Effective collision strength at 7x10^6 K --- U08 Effective collision strength at 8x10^6 K --- U09 Effective collision strength at 9x10^6 K --- U10 Effective collision strength at 10^7 K --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Mar 10 Alberto Maria Binello <A.M.Binello@damtp.cam.ac.uk> J_A+AS_131_153.xml F, G and K stars in the ROSAT all-sky survey. I. Photometry. J/A+AS/131/197 J/A+AS/131/197 F, G and K stars BVRI photometry F, G and K stars in the ROSAT all-sky survey. I. Photometry. A D F Metanomski L Pasquini J Krautter G Cutispoto T A Fleming Astron. Astrophys. Suppl. Ser. 131 197 1998 1998A&AS..131..197M IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) IX/15 : Einstein EMSS Survey (Gioia+ 1990, Stocke+ 1991) J/ApJS/99/701 : EMSS (Fleming+ 1995) J/A+AS/115/41 : UBV(RI) photometry of cool stars (Cutispoto+, 1996) Photometry, UBVRI Radio sources Stars, late-type stars: late-type surveys X-rays: stars We present accurate BV(RI)c photometry for a sample of F, G and K stars detected in selected areas of the ROSAT all-sky survey (RASS). We have used the photometry, in addition to low-resolution spectroscopy, to estimate spectral classifications, distances and X-ray luminosities. The log(L_X_/L_V_) in the sample lies below -2. Although the sample contains also nearby, inactive stars, it is dominated by active objects. The median X-ray luminosity in our sample is <L_X_>=29.88 and the mean value of the hardness ratios <HR1>=0.13+/-0.35. We compare the derived X-ray luminosity function with similar functions obtained from the serendipitous samples of the Einstein Observatory medium sensitivity survey (EMSS, Cat. <IX/15>) and EXOSAT (Cat. <J/A+AS/115/41>). Our sample is completely consistent with the EMSS sample of solar type stars, indicating that both our sources and the EMSS sources are representative of the high galactic latitude X-ray stellar population. We do not find extremely active stars (log(L_X_)>=32), as are found in the EMSS sample, and we argue that these objects are rare.
ROSAT
Summary of X-ray and observational data as well as results for the studied sample RXJ ROSAT name --- n_RXJ *: see note detailed in file notes.dat --- RAXh X-ray source right ascension (2000.0) h RAXm X-ray source right ascension (2000.0) min RAXs X-ray source right ascension (2000.0) s DEX- X-ray source declination sign --- DEXd X-ray source declination (2000.0) deg DEXm X-ray source declination (2000.0) arcmin DEXs X-ray source declination (2000.0) arcsec Counts Count-rate for the X-ray source ct/s Texp Total exposition time s HR1 Hardness Ratio 1 number=1 HR1 = (CR[ch52-201]-CR[ch11-41])/CR[ch11-240] where CD[cha-b] being the count-rate in the channels "a" to "b" --- RAh Counterpart right ascension (2000.0) h RAm Counterpart right ascension (2000.0) min RAs Counterpart right ascension (2000.0) s DE- Counterpart declination sign --- DEd Counterpart declination (2000.0) deg DEm Counterpart declination (2000.0) arcmin DEs Counterpart declination (2000.0) arcsec DX-C Distance between X-ray and counterpart positions arcsec SpType Spectral type --- n_SpType Note on Spectral type for binaries number=2 1: the binarity/multiplicity obtained by the photometry was confirmed by the high-resolution spectra 2: the binarity was determined for the high-resolution spectra 3: the binarity is a visual one 4: the binarity information was only obtained through the literature --- Dist Distance of the star form the Sun pc E_Dist Error in Distance (upper limit) pc e_Dist Error in Distance (lower limit) pc fX X-ray flux 10-15W/m2 E_fX Error in fX (upper limit) 10-15W/m2 e_fX Error in fX (lower limit) 10-15W/m2 LX X-ray luminosity 10+22W E_LX Error in LX (upper limit) 10+22W e_LX Error in Lx (lower limit) 10+22W Name Counterpart name --- SpTypeO Counterpart spectral type --- Vmag Counterpart V magnitude mag B-V Counterpart B-V colour index mag V-R Counterpart V-R colour index mag V-I Counterpart V-I colour index mag Individual notes RXJ Source name --- Ntot Total number of lines for the RXJ object --- Nline Running line number in range [1,Ntot] --- Note Text of the note --- Patricia Bauer CDS 1998 Jul 31 UNKNOWN UNKNOWN Prepared via OCR at CDS An error was detected in the original publication and corrected. For RXJ 1413.7-0050, the position of the Counterpart (HD 124425) is 14 13 40.6 -00 50 40 instead of 14 13 40.6 -00 05 40 J_A+AS_131_197.xml Distances to five resolved galaxies in the CVn cloud J/A+AS/131/1 J/A+AS/131/1 BVI photometry of 5 CVn cloud galaxies Distances to five resolved galaxies in the CVn cloud I D Karachentsev I O Drozdovsky Astron. Astrophys. Suppl. Ser. 131 1 1998 1998A&AS..131....1K J/A+AS/124/559 : VI photometry of dwarf galaxies (Karanchentsev+ 1997) J/A+AS/128/459 : BV photometry of irregular galaxies (Makarova+ 1998) Galaxies, photometry galaxies: distances and redshifts galaxies: individual (NGC 4144, NGC 4244, NGC 4395, NGC 4449) galaxies: individual (UGC 8331) galaxies: nearby We present results of CCD imaging in B, V of five late-type galaxies with radial velocities V_0_<350km/s in the Canes Venatici cloud. Based on the photometry of their brightest blue stars we derived the following distances to the galaxies: 9.7Mpc for NGC 4144, 4.5Mpc for NGC 4244, 4.2Mpc for NGC 4395, 2.9Mpc for NGC 4449, and 8.2Mpc for UGC 8331.
NGC 4144 UGC 7151 12 09.9 +46 26 NGC 4244 UGC 7322 12 17.5 +37 48 NGC 4395 UGC 7524 12 25.9 +33 32 NGC 4449 UGC 7592 12 28.2 +44 05 UGC 8331 13 15.5 +47 29
BVI photometry (table3 to table7) Gal Galaxy name --- m_Gal Multiplicity index on Gal --- Star Star number --- Xpos Rectangular coordinates of stars number=1 The upper right corner corresponds to X=0, Y=0 of the frame coordinates given in the Tables 3-7, i.e. X increases to East and Y to South. pix Ypos Rectangular coordinates of stars number=1 The upper right corner corresponds to X=0, Y=0 of the frame coordinates given in the Tables 3-7, i.e. X increases to East and Y to South. pix Vmag V magnitude mag B-V (B-V) colour index mag V-I (V-I) colour index mag SHAR Image parameter SHAR --- Patricia Bauer CDS 1998 Jan 09 Korotkova G.G <ggk@luna.sao.ru> J_A+AS_131_1.xml Broad-band JHK(L') photometry of a sample of giants with 0.5>[Fe/H]>-3 J/A+AS/131/209 J/A+AS/131/209 JHK Broad-band JHK(L') photometry of a sample of giants with 0.5>[Fe/H]>-3 A Alonso S Arribas C Martinez-Roger Astron. Astrophys. Suppl. Ser. 131 209 1998 1998A&AS..131..209A J/A+AS/107/365 : Dwarfs and subdwarfs IR photometry (Alonso+, 1994) J/A+AS/117/227 : Dwarf effective temperatures (Alonso+ 1996) Photometry, infrared Stars, giant infrared: stars stars: fundamental parameters stars: general stars: Population II We present the results of a three-year campaign of broad-band photometry in the near-infrared J, H, K and L' bands for a sample of approximately 250 giant stars carried out at the Observatorio del Teide (Tenerife, Spain). Transformations of the Telescopio Carlos Sanchez system into/from several currently used infrared systems are extended to the redward part of the colour axis. The linearity of our photometric system in the range -3mag<K<10.5mag is inferred from the intercomparison of data of stars common to this and other photometric systems. A preliminary assessment of the photometric extinction profile of the Observatorio del Teide in JHKL' is also provided. These observations are a continuation of a programme aimed towards the progressive completion of a whole grid of T_eff_-[Fe/H]-log(g)-colour relations for population I and II stars. The analysis of optical and IR colour-colour diagrams reveals that the range F0III-K5III is well sampled for 0.5>[Fe/H]>-3. Data of comparable quality previously published have been added to the sample in order to increase the reliability of the relations to be obtained. We also provide mean IR colours for giant stars according to spectral type.
Infrared photometric magnitudes of the calibrating stars measured at the Observatorio del Teide (Carlos Sanchez Telescope; TCS) during this programme of observations. Name BS (Cat. <V/50>) or SAO (Cat. <I/131>) name --- Jmag J magnitude mag e_Jmag rms uncertainty on Jmag mag o_Jmag Number of observations in Jmag --- --- --- o2_Jmag Number of observations in Jmag --- Hmag H magnitude mag e_Hmag rms uncertainty on Hmag mag o_Hmag Number of observations in Hmag --- --- --- o2_Hmag Number of observations in Hmag --- Kmag K magnitude mag e_Kmag rms uncertainty on Kmag mag o_Kmag Number of observations in Kmag --- --- --- o2_Kmag Number of observations in Kmag --- L'mag L' magnitude mag e_L'mag rms uncertainty on L'mag mag o_L'mag Number of observations in L'mag --- --- --- o2_L'mag Number of observations in L'mag --- SpType Spectral type --- Photometric data measured with the Carlos Sanchez Telescope (TCS) at the Observatorio del Teide. Name Star name --- n_Name Note on Name number=1 1: Variable: V352 Aur 2: Variable ? 3: Binary system separated 4.5" 4: Binary system 5: Variable ? 6: Misidentification ? 7: Unidentified star measured in the field of SAO 144547 --- Jmag J magnitude mag e_Jmag rms uncertainty on Jmag mag o_Jmag Number of observations in Jmag --- Hmag H magnitude mag e_Hmag rms uncertainty on Hmag mag o_Hmag Number of observations in Hmag --- Kmag K magnitude mag e_Kmag rms uncertainty on Kmag mag o_Kmag Number of observations in Kmag --- L'mag L' magnitude mag e_L'mag rms uncertainty on L'mag mag o_L'mag Number of observations in L'mag --- SpType Spectral type --- *Normalized filter transmission for L' band, where the sensitivity of the InSb detector has been included. Lambda Wavelength nm T Normalized transmission. --- Patricia Bauer CDS 1998 Jun 15 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_131_209.xml Kinematics of the southern galaxy cluster Abell 3733 J/A+AS/131/221 J/A+AS/131/221 Abell 3733 radial velocities Kinematics of the southern galaxy cluster Abell 3733 J M Solanes P Stein Astron. Astrophys. Suppl. Ser. 131 221 1998 1998A&AS..131..221S Clusters, galaxy Radial velocities galaxies: clusters: individual (A 3733) galaxies: distances and redshifts Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.
MEFOS and OPTOPUS multifiber spectra velocities for A3733 RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec bj b_j magnitude mag HRVccM Cross-correlation heliocentric radial velocity from MEFOS km/s e_HRVccM Estimated external error on HRVccM km/s HRVelM Emission-line heliocentric radial velocity from MEFOS km/s e_HRVelM Estimated external error on HRVelM km/s HRVccO Cross-correlation heliocentric radial velocity from OPTOPUS km/s e_HRVccO Estimated external error on HRVccO km/s HRVelO Emission-line heliocentric radial velocity from OPTOPUS km/s e_HRVelO Estimated external error on HRVelO km/s HRVa Average heliocentric radial velocity km/s e_HRVa Estimated external error on HRVa km/s J.M. Solanes U. of Barcelona 1998 Mar 04 Jose-Maria Solanes <solanes@pcess1.am.ub.es> J_A+AS_131_221.xml The overlapping open clusters NGC 1750 and NGC 1758: II. BVR photographic photometry and proper motions J/A+AS/131/239 J/A+AS/131/239 NGC 1750 + NGC 1758 BVR photometry The overlapping open clusters NGC 1750 and NGC 1758: II. BVR photographic photometry and proper motions D Galadi-Enriquez C Jordi E Trullols J Guibert K -P Tian J -L Zhao Astron. Astrophys. Suppl. Ser. 131 239 1998 1998A&AS..131..239G J/A+A/333/471 : UBVRI photometry of NGC 1750 & NGC 1758 (Galadi-Enriquez+ 1998) J/A+AS/131/89 : NGC 1750 + NGC 1758 proper motions (Tian+ 1998) I/149 : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) - Extension (Fricke+ 1991) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Arias et al., The extragalactic reference system of the International Earth Rotation Service, ICRS. (1995A&A...303..604A) Galadi-Enriquez et al., Paper III 1998A&A...337..125G Clusters, open Photometry, UBVRI Proper motions astrometry open clusters and associations: individual (NGC 1746, NGC 1750) open clusters and associations: individual (NGC 1758) Photographic astrometric and photometric catalogue. Table 6 contains (x,y) positions, (mu_x, mu_y) relative proper motions and BVR photographic photometry. Notes give cross-identifications with other catalogues. Table 11 contains equatorial positions (alpha, delta) and absolute proper motions (mu_alpha cos delta, mu_delta) in FK5 and ICRS reference systems.
NGC 1746 C 0500+237 05 03.6 +23 49 NGC 1750 C 0500+235 05 03.9 +23 39 NGC 1758 C 0501+237 05 04.4 +23 47
Photographic photometric and astrometric catalogue Ident Identification --- xpos x coordinate (master plate ref. system) number=1 Coordinates xpos and ypos include the {xi} and {eta} parameters (Eqs. 6 and 7) for stars with computed proper motions. The error of xpos and ypos coordinates are that of {xi} and {eta} parameters for stars with proper motions computed from more than three plates. An error of 99.99 microns is quoted for stars without proper motion, or with proper motion computed fom only two plates. mm ypos y coordinate (master plate ref. system) number=1 Coordinates xpos and ypos include the {xi} and {eta} parameters (Eqs. 6 and 7) for stars with computed proper motions. The error of xpos and ypos coordinates are that of {xi} and {eta} parameters for stars with proper motions computed from more than three plates. An error of 99.99 microns is quoted for stars without proper motion, or with proper motion computed fom only two plates. mm pmxpos Relative proper motion along x number=2 Proper motions of 99.99 mas/yr are quoted for stars without proper motion available. Proper motion errors of 99.99 mas/yr are assigned to stars without proper motion, or with proper motion computed from only two plates. mas/yr pmypos Relative proper motion along y number=2 Proper motions of 99.99 mas/yr are quoted for stars without proper motion available. Proper motion errors of 99.99 mas/yr are assigned to stars without proper motion, or with proper motion computed from only two plates. mas/yr e_xpos Error of x coordinate number=1 Coordinates xpos and ypos include the {xi} and {eta} parameters (Eqs. 6 and 7) for stars with computed proper motions. The error of xpos and ypos coordinates are that of {xi} and {eta} parameters for stars with proper motions computed from more than three plates. An error of 99.99 microns is quoted for stars without proper motion, or with proper motion computed fom only two plates. um e_ypos Error of y coordinate number=1 Coordinates xpos and ypos include the {xi} and {eta} parameters (Eqs. 6 and 7) for stars with computed proper motions. The error of xpos and ypos coordinates are that of {xi} and {eta} parameters for stars with proper motions computed from more than three plates. An error of 99.99 microns is quoted for stars without proper motion, or with proper motion computed fom only two plates. um e_pmxpos Error of proper motion in x mas/yr e_pmypos Error of proper motion in y mas/yr Bmag Johnson B photographic magnitude number=3 Stars having B and R values, but lacking V photometry, are assigned Vmag=99.99 mag. Stars lacking standard photographic photometry are assigned Bmag=99.99 mag, Vmag=99.99 mag and, if available, the R value from the master plate raw photometric photometry for cross- identifications (Sect. 3.3) is given as the best estimation of R magnitude. Bright stars lacking photometry due to saturation are assigned Bmag=Vmag=Rmag=0.00 mag. For the photometric errors, see Table 4 and Fig. 2. mag Vmag Johnson V photographic magnitude number=3 Stars having B and R values, but lacking V photometry, are assigned Vmag=99.99 mag. Stars lacking standard photographic photometry are assigned Bmag=99.99 mag, Vmag=99.99 mag and, if available, the R value from the master plate raw photometric photometry for cross- identifications (Sect. 3.3) is given as the best estimation of R magnitude. Bright stars lacking photometry due to saturation are assigned Bmag=Vmag=Rmag=0.00 mag. For the photometric errors, see Table 4 and Fig. 2. mag Rmag Cousins R photographic magnitude number=3 Stars having B and R values, but lacking V photometry, are assigned Vmag=99.99 mag. Stars lacking standard photographic photometry are assigned Bmag=99.99 mag, Vmag=99.99 mag and, if available, the R value from the master plate raw photometric photometry for cross- identifications (Sect. 3.3) is given as the best estimation of R magnitude. Bright stars lacking photometry due to saturation are assigned Bmag=Vmag=Rmag=0.00 mag. For the photometric errors, see Table 4 and Fig. 2. mag Nplate Number of plates for proper motion calculation --- delta(t) Maximum epoch difference with master plate for proper motion calculation yr List of 1713 stars cross-identified with other catalogues Ident Identification --- --- --- Names Other names, separated by a comma number=1 The codes used are: TYC: Tycho Catalogue, ESA, 1997, ESA-SP 1200, Cat. <I/239> HIP: Hipparcos Catalogue, ESA, 1997, ESA-SP 1200, Cat. <I/239> PPM: Positions and Proper Motions Catalogue, Roeser and Bastian, 1989, Cat. <I/146> and <I/193> HD: Henry Draper Catalogue, Cat. <III/135> BD: Bonner Durchmusterung, Cat. <I/122> GJTR: Paper I, Galadi-Enriquez et al., Cat. <J/A+A/333/471> SChM: Straizhys, Chernis and Meishtas, 1992BaltA...1..125S, [SCM92b] NNN in SIMBAD Cuf: Cuffey, 1937AnHar.105..403C --- FK5 and ICRS positions and proper motions Ident Identification --- RAJh FK5 right ascension, ep. 1994.9, eq. J2000 h RAJm FK5 right ascension, ep. 1994.9, eq. J2000 min RAJs FK5 right ascension, ep. 1994.9, eq. J2000 s DEJ- Sign of FK5 declination --- DEJd FK5 declination, ep. 1994.9, eq. J2000 deg DEJm FK5 declination, ep. 1994.9, eq. J2000 arcmin DEJs FK5 declination, ep. 1994.9, eq. J2000 arcsec pmRAJ FK5 proper motion in alpha*cos(delta) mas/yr pmDEJ FK5 proper motion in delta mas/yr RAh ICRS right ascension, ep. 1994.9 h RAm ICRS right ascension, ep. 1994.9 min RAs ICRS right ascension, ep. 1994.9 s DE- Sign of ICRS declination --- DEd ICRS declination, ep. 1994.9 deg DEm ICRS declination, ep. 1994.9 arcmin DEs ICRS declination, ep. 1994.9 arcsec pmRA ICRS proper motion in alpha*cos(delta) mas/yr pmDE ICRS proper motion in delta mas/yr Patricia Bauer CDS 1998 Mar 10 David Galadi-Enriquez <dgaladi@pchpc5.am.ub.es> UNKNOWN UNKNOWN * 10-Mar-1998: first version * 09-Sep-1998: table11 was corrected by the author (13 stars has a missing sign in the proper motion) J_A+AS_131_239.xml Kinematical data on early-type galaxies. IV. J/A+AS/131/287 J/A+AS/131/287 Kinematical data on early-type galaxies. IV. Kinematical data on early-type galaxies. IV. F Simien P Prugniel Astron. Astrophys. Suppl. Ser. 131 287 1998 1998A&AS..131..287S J/A+AS/122/521 : Kinematical data on early-type galaxies. I. (Simien+ 1997) J/A+AS/126/15 : Kinematical data on early-type galaxies. II. (Simien+ 1997) J/A+AS/126/519 : Kinematical data on early-type galaxies. III. (Simien+ 1997) Galaxies, rotation Radial velocities Velocity dispersion galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: general galaxies: kinematics and dynamics We present kinematical data for a sample of 25 galaxies. Rotation curves and velocity-dispersion profiles are determined for 16 objects, while the central velocity dispersions are given for the whole sample. This is our fourth paper in a series devoted to the presentation of kinematical data on elliptical and S0 galaxies, derived from long-slit absorption spectroscopy.
Catalog elements and kinematical results Name Object identification --- Mtype Morphological type --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Bt Integrated blue magnitude mag m-M Distance modulus mag Re Effective radius arcsec Eps Ellipticity --- PA Position angle of slit PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). deg r_Eps Reference for Eps and PA 1 = Djorgovski (1985, PhD thesis. Univ. of California, Berkeley) 2 = Michard & Marchal (1993A&AS...98...29M) 3 = LEDA (status: LEDA1997). --- Vhel Heliocentric radial velocity km/s u_Vhel Uncertainty flag on Vhel --- e_Vhel Mean error on Vhel km/s sig0 Central velocity dispersion km/s u_sig0 Uncertainty flag on sig0 Uncertainty due to bad seeing conditions. --- e_sig0 Mean error on sig0 km/s l_Vmax Upper- or lower-limit flag on Vmax --- Vmax Maximum rotational velocity km/s u_Vmax Uncertainty flag on Vmax --- e_Vmax Mean error on Vmax km/s rmax Radius corresponding to Vmax arcsec Log of the observations Name Object identification --- Date Date of observation "DD/MM/YY" Setup Spectrograph setup Setup=1 corresponds to a dispersion of 66{AA}/mm Setup=2 corresponds to a dispersion of 33{AA}/mm --- PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with the following convention on the subsequent radius r in the profiles (Table 3): - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg Nexp Number of exposures --- Texp Exposure time min Seeing Seeing FWHM arcsec u_Seeing Uncertainty flag on Seeing --- Profiles of velocity dispersion and rotation Name Object identification --- PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg r Radius (<0 and >0 on opposite semi-axes) arcsec Vrot Proj. mean stellar rotation velocity Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. km/s e_Vrot Mean error on V km/s sigma Projected velocity dispersion km/s e_sigma Mean error on sigma km/s Patricia Bauer CDS 1998 Jun 09 Francois Simien <simien@obs.univ-lyon1.fr> J_A+AS_131_287.xml New CCD positions of Triton and a comparison with the theoretical predictions J/A+AS/131/291 J/A+AS/131/291 1995-1997 CCD positions of Triton New CCD positions of Triton and a comparison with the theoretical predictions C H Veiga R Vieira Martins Astron. Astrophys. Suppl. Ser. 131 291 1998 1998A&AS..131..291V J/A+AS/120/107 : 1989-1994 CCD observations of Triton (Veiga+ 1996) Planets Positional data astrometry planets and satellites: individual (Triton) Astrometric observations of Triton are given for the oppositions of Neptune on 1995, 1996 and two nights of 1997. In this period, 759 frames were obtained during 35 nights at the Cassegrain focus of the 1.6m and the 0.6m reflectors of the LNA-Brazil. The comparison with calculated positions gives residuals with standard deviation of the order of 0.09".
List of observed positions of the Neptunian satellite Obs.Y Mean instant of the observation (year) yr Obs.M Mean instant of the observation (month) --- Obs.d Mean instant of the observation (day) d Sat Nema of the satellite --- DRA {DELTA}{alpha}cod{delta} position relative to Neptune (J2000) arcsec DDE {DELTA}{delta} position relative to Neptune (J2000) arcsec Patricia Bauer CDS 1998 Mar 09 Carlos Henrique Veiga <cave@dans.on.br> J_A+AS_131_291.xml Spectral survey of Case emission-line galaxies with the 6m Russian telescope J/A+AS/131/295 J/A+AS/131/295 Spectral survey of Case emission-line galaxies Spectral survey of Case emission-line galaxies with the 6m Russian telescope A V Ugryumov S A Pustilnik V A Lipovetsky Yu I Izotov G Richter Astron. Astrophys. Suppl. Ser. 131 295 1998 1998A&AS..131..295U J/AJ/109/2376 : Case survey blue/emission-line galaxies (Salzer+ 1995) J/ApJS/66/309 : Case low-dispersion Survey VI. (Sanduleak 1988) J/ApJS/66/387 : Case low-dispersion Survey VII. (Sanduleak+ 1988) J/ApJS/71/549 : Case low-dispersion Survey X. (Pesch+ 1989) J/ApJS/86/453 : Case Low-Dispersion Survey XIV. (MacConnell+ 1993) 1 1985Thesi.........L Lipovetsky SAO RAS 2 1989SoSAO..62....5M Markarian et al. Cat. <VII/172> 3 1986ApJS...62..751M Mazzarella & Balzano 4 1986ApJS...60..543P Pesch & Sanduleak Paper III 5 1988ApJS...66..297P Pesch & Sanduleak Paper V 6 1989ApJS...70..163P Pesch & Sanduleak Paper VIII 7 1991ApJS...76.1043P Pesch, et al. Paper XII 8 1989ApJS...70..479S Salzer et al. 9 1982ApJ...258L..11S Sanduleak & Pesch 10 1984ApJS...55..517S Sanduleak & Pesch Paper II 11 1987ApJS...63..809S Sanduleak & Pesch Paper IV 12 1989ApJS...70..173S Sanduleak & Pesch Paper IX 13 1990ApJS...72..291S Sanduleak & Pesch Paper XI Galaxies, spectra Galaxy catalogs Radial velocities galaxies: compact galaxies: distances and redshifts galaxies: fundamental parameters galaxies: starburst surveys The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.
Coordinates, velocities and magnitudes of ELGs Note Object observed with CCD number=1 Mark '*' for objects observed with CCD --- Name Name of objects number=2 Names from the Case and Markarian catalogs, refs 1-7, 9-13 in "References" section below --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Pmag Photographic magnitude number=3 Photographic magnitudes from the Case and Markarian catalogs, refs 1-7, 9-13 in "References" section below mag HRV Heliocentric radial velocity km/s u_HRV Uncertainty flag on HRV number=4 Mark ':' for less accurate heliocentric velocities --- PMag Absolute photographic magnitude mag Names Other names from NED --- Spectral parameters of ELGs Note Object observed with CCD number=1 Mark '*' for objects observed with CCD --- Name Name of objects number=2 Names from the Case and Markarian catalogs, refs. 1-7, 9-13 in "References" section below --- IUE IUE name of objects --- Code Code about [OIII] emission number=3 Eye estimates of the strength of the blended emission lines of [OIII]4959,5007A taken from the Case survey, refs. 4-7,9-13 in "References" section below --- OII/Hbeta Emission line fluxes ratio [OII]3727{AA}/Hbeta --- OIII/Hbeta Emission line fluxes ratio [OIII]5007{AA}/Hbeta --- EWHbeta Equivalent width of Hbeta emission line 0.1nm EW[OII] Equivalent width of [OII]3727{AA} emission line 0.1nm u_EW[OII] Uncertainty flag on EW[OII] number=4 Mark ':' for less accurate measured equivalent widths --- EW[OIII] Equivalent width of [OIII]5007{AA} emission line 0.1nm u_EW[OIII] Uncertainty flag on EW[OIII] number=4 Mark ':' for less accurate measured equivalent widths --- Type Spectral Type number=5 Only rough classification were done due to low S/N spectra. Spectral classification follows Salzer et al. (1989ApJS...70..479S) --- Objects with non-detected emission lines Note Object observed with CCD number=1 Mark '*' for objects observed with CCD --- Name Name of objects number=2 Names from the Case and Markarian catalogs, refs 1-7, 9-13 in "References" section below --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Pmag Photographic magnitude number=3 Photographic magnitudes from the Case and Markarian catalogs, refs 1-7, 9-13 in "References" section below mag HRV Heliocentric radial velocity km/s u_HRV Uncertainty flag on HRV number=4 Mark ':' for less accurate heliocentric velocities --- PMag Absolute photographic magnitude mag Code Code about [OIII] emission number=5 Eye estimates of the strength of the blended emission lines of [OIII]4959,5007A taken from the Case survey references, refs 4-7, 9-13 in "References" section below --- Features Detected spectral features number=6 Due to low S/N level no features in some spectra were identified. These objects are marked as having inconclusive spectra (inc.) --- Names Other names from NED --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 May 29 Andrew Ugryumov <and@relay.sao.ru> J_A+AS_131_295.xml A complete sample of GHz-Peaked-Spectrum radio sources and its radio properties J/A+AS/131/303 J/A+AS/131/303 GHz-Peaked-Spectrum radio sources A complete sample of GHz-Peaked-Spectrum radio sources and its radio properties C Stanghellini C P O'Dea D Dallacasa S A Baum R Fanti C Fanti Astron. Astrophys. Suppl. Ser. 131 303 1998 1998A&AS..131..303S VIII/42 : Texas Survey of radio sources at 365MHz (Douglas+ 1996) VIII/16 : Molonglo Reference Catalogue of Radio Sources (Large+ 1991) VIII/5 : Bright Extragalactic Radio Sources (1Jy) (Kuehr+, 1981) VIII/37 : The Third Bologna Survey (B3) (Ficarra+ 1985) VIII/18 : 6C Survey of radio sources I. (Baldwin+ 1985) VIII/21 : 6C Survey of radio sources II. (Hales+ 1988) VIII/22 : 6C Survey of Radio Sources III. (Hales+ 1990) VIII/23 : 6C Survey of radio sources IV. (Hales+ 1991) VIII/24 : 6C Survey of Radio Sources V. (Hales+ 1993) VIII/25 : 6C Survey of radio sources VI. (Hales+ 1993) Radio sources galaxies: active quasars: general radio continuum: galaxies We define a complete sample of thirty-three GHz-Peaked-Spectrum (GPS) radio sources based on their spectral properties. We present measurements of the radio spectra and polarization of the complete sample and a list of additional GPS sources which fail one or more criteria to be included in the complete sample. The majority of the data have been obtained from quasi-simultaneous multi-frequency observations at the Very Large Array (VLA) during 3 observing sessions. Low frequency data from the Westerbork Synthesis Radio Telescope (WSRT) and from the literature have been combined with the VLA data in order to better define the spectral shape. The objects presented here show a rather wide range of spectral indices at high and low frequencies, including a few cases where the spectral index below the turnover is close to the theoretical value of 2.5 typical of self-absorbed incoherent synchrotron emission. Faint and diffuse extended emission is found in about 10% of the sources. In the majority of the GPS sources, the fractional polarization is found to be very low, consistent with the residual instrumental polarization of 0.3%.
Flux densities for the complete sample Flux densities for the additional objects Name Source Name number=1 Individual notes: 0108+388: the flux density at 608 MHz and higher frequencies refers to the core only, while the flux density measure at 325 MHz likely includes the extended structure found close to the main compact component (Baum et al. 1990). 0552+398: the flux density at 37 GHz is the average of the data taken in 1990 (Terasranta et al., 1992A&AS...94..121T), and the error is the r.m.s of the distribution. The flux density at 90GHz is the average of the data taken in 1990 (Steppe et al., 1992A&AS...96..441S), and the error is the r.m.s of the distribution. 2134+004: The flux density at 87 GHz is the average of the data taken between 1985 and 1988 (Terasranta et al., 1992A&AS...94..121T), the error is the r.m.s of the distribution. --- nu Frequency GHz Snu Flux density Jy e_Snu rms uncertainty on S number=2 The errors are taken as 3% if they were found in literature to be less then 3%. Jy r_Snu References number=3 1: VLA first session 2: VLA second session 3: VLA third session 4: WSRT 5: Northern Cross 6: Ratan 600 7: Douglas et al., 1996AJ....111.1945D, Cat. <VIII/42> 8: Large et al., 1981MNRAS.194..693L, Cat. <VIII/16> 9: Kuhr et al., 1981A&AS...45..367K, Cat. <VIII/5> 10: Baum et al., 1990A&A...232...19B 11: de Bruyn, private communication 12: de Bruyn, 1990, in Proc. Dwingeloo Workshop, Compact Steep Spectrum and GHz Peaked Spectrum Radio Sources, ed. C. Fanti, R.Fanti, C.P. O'Dea, & R.T. Schilizzi, (Bologna: Istituto di Radioastronomia), p.105 13: Steppe et al., 1988A&AS...75..317S 14: Chandler, 1995, VLA Test Memo 192 15: Ficarra et al., 1985A&AS...59..255F, Cat. <VIII/37> 16: Esko, private communication 17: Gower et al., 1967MmRAS..71...49G, Pilkington et al., 1965MmRAS..69..183P 18: Dennison et al., 1981AJ.....86.1604D 19: Edelson, 1987AJ.....94.1150E 20: Terasranta et al., 1992A&AS...94..121T 23: Fiedler et al., 1987ApJS...65..319F 24: Steppe et al., 1992A&AS...96..441S 25: Baldwin et al., 1985MNRAS.217..717B, Cat. <VIII/18> 26: Hales et al., 1988MNRAS.234..919H, Cat. <VIII/21> 27: Hales et al., 1990MNRAS.246..256H, Cat < VIII/22> 28: Hales et al., 1991MNRAS.251...46H, Cat. <VIII/23> 29: Hales et al., 1993MNRAS.262.1057H, Cat. <VIII/24> 30: Hales et al., 1993MNRAS.263...25H, Cat. <VIII/25> 31: Khabrakhmanov, private communication. --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1998 Mar 19 Carlo Stanghellini <cstan@stsci.edu> J_A+AS_131_303.xml Catalogue of HII regions in NGC 7331 at the 6 meter telescope J/A+AS/131/317 J/A+AS/131/317 NGC 7331 HII regions catalogue Catalogue of HII regions in NGC 7331 at the 6 meter telescope H Petit Astron. Astrophys. Suppl. Ser. 131 317 1998 1998A&AS..131..317P J/A+A/268/419 : HII Regions in NGC 4258 (Courtes+ 1993) J/A+A/309/446 : HII Regions in M51 (Petit+, 1996) J/A+AS/131/319 : HII Regions catalogue (Petit+ 1998) H II regions Positional data catalogs galaxies: ISM HII regions A catalogue of HII regions in NGC 7331 is presented, with positions relative to the center of the Galaxy and relative H{alpha} fluxes.
NGC 7331 HII regions catalogue Galaxy Name of the galaxy (NGC 7331) --- Object Object number number=1 Origin of the HII regions numbers: M33: Boulesteix et al., 1974A&A....37...33B, for number 1-1502 (<BCLMP NNNNA>) Courtes et al., 1987A&A...174...28C, for number Z1-Z410 (<CPSDP NNNA>) M51: Petit et al., 1996, Cat. <J/A+A/309/446> (<[PHB96] NNN>) M81: Petit et al., 1988A&AS...74..475P (<PSK NNN>) NGC 2403: Sivan et al., 1990A&A...237...23S (<[SPC90] NNN>) NGC 4258: Courtes et al., 1993, Cat. <J/A+A/268/419> ([CPH93]) NGC 7331: This paper --- RAh Right ascension (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. h RAm Right ascension (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. min RAs Right ascension (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. s DE- Declination sign --- DEd Declination (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. deg DEm Declination (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. arcmin DEs Declination (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. arcsec Xpos X value referred to galaxy centre (4) number=3 Xpos and Ypos are axes ib the E-W and N-S directions respectively. arcsec Ypos Y value referred to galaxy centre (4) number=3 Xpos and Ypos are axes ib the E-W and N-S directions respectively. arcsec FHa H{alpha} flux value number=4 No data for M 33. 10-19W/m2 n_FHa *: FHa is not an absolute flux --- DiamEff Effective diameter number=4 No data for M 33. arcsec DiamGeo Geometric diameter number=4 No data for M 33. arcsec logL Log Luminosity number=4 No data for M 33. [10-7W] xdim x dimension of HII region (for M33 only) arcsec ydim y dimension of HII region (for M33 only) arcsec Patricia Bauer CDS 1998 Apr 23 H. Petit, Observatoire de Marseille, F13248 Marseille Cedex 04 UNKNOWN UNKNOWN In order to homogenize the presentation, we made approximations on all data so that the catalogue is easily readable. If one needs more accurate data one can look at the original publication. For the galaxy NGC 7331, the photographic densities are converted into arbitrary intensities using a relative photometric calibration. J_A+AS_131_317.xml Catalogue of HII regions measured on 6m telescope plates at Observatoire de Marseille J/A+AS/131/319 J/A+AS/131/319 HII regions catalogue Catalogue of HII regions measured on 6m telescope plates at Observatoire de Marseille H Petit P Figon M Petit Astron. Astrophys. Suppl. Ser. 131 319 1998 1998A&AS..131..319P J/A+A/268/419 : HII Regions in NGC 4258 (Courtes+ 1993) J/A+A/309/446 : HII Regions in M51 (Petit+, 1996) J/A+AS/131/317 : NGC 7331 HII regions catalog (Petit 1998) H II regions Positional data catalogs galaxies: ISM HII regions Several galaxies were studied at Observatoire de Marseille using the films obtained at the 6 m telescope with the Great Focal Reducer installed at the prime focus of the russian telescope. We thought that before we retire, it should be of some interest for the astronomical community to find in a single catalogue all the data we published to facilitate the research. (see hereunder the references). We give in this catalogue the data of the following galaxies: M 33, M 51, M 81, NGC 2403, NGC 4258 and NGC 7331. NGC 4258 was not studied with the 6 m telescope, but we added its results because it was published by the same team using the same softwares. For NGC 7331 (see Petit 1998, Cat. <J/A+AS/131/317>). The flux values are followed by*; that means that they are not absolute fluxes like in the other publications. In order to make the catalogue easier to consult, we homogeneised the data. So, one can find some slight differences between the original data and the catalogue ones. The details of these modifications are precised in the Readme file associated to the catalogue in the data base. We did not keep the remarks so it is necessary to look at the original publication to find the full information. We give the whole references hereunder to facilitate the research of the original articles.
HII regions catalogue Galaxy Name of the galaxy --- Object Object number number=1 Origin of the HII regions numbers: M33: Boulesteix et al., 1974A&A....37...33B, for number 1-1502 (<BCLMP NNNNA>) Courtes et al., 1987A&A...174...28C, for number Z1-Z410 (<CPSDP NNNA>) M51: Petit et al., 1996, Cat. <J/A+A/309/446> (<[PHB96] NNN>) M81: Petit et al., 1988A&AS...74..475P (<PSK NNN>) NGC 2403: Sivan et al., 1990A&A...237...23S (<[SPC90] NNN>) NGC 4258: Courtes et al., 1993, Cat. <J/A+A/268/419> ([CPH93]) NGC 7331: This paper --- RAh Right ascension (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. h RAm Right ascension (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. min RAs Right ascension (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. s DE- Declination sign --- DEd Declination (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. deg DEm Declination (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. arcmin DEs Declination (1950) number=2 Position of the galaxy centre, expect for M33, where the position is that of the HII region. arcsec Xpos X value referred to galaxy centre (4) number=3 Xpos and Ypos are axes ib the E-W and N-S directions respectively. arcsec Ypos Y value referred to galaxy centre (4) number=3 Xpos and Ypos are axes ib the E-W and N-S directions respectively. arcsec FHa H{alpha} flux value number=4 No data for M 33. 10-19W/m2 n_FHa *: FHa is not an absolute flux --- DiamEff Effective diameter number=4 No data for M 33. arcsec DiamGeo Geometric diameter number=4 No data for M 33. arcsec logL Log Luminosity number=4 No data for M 33. [10-7W] xdim x dimension of HII region (for M33 only) arcsec ydim y dimension of HII region (for M33 only) arcsec Patricia Bauer CDS 1998 Apr 23 H. Petit, Observatoire de Marseille, F13248 Marseille Cedex 04 UNKNOWN UNKNOWN In order to homogenize the presentation, we made approximations on all data so that the catalogue is easily readable. If one needs more accurate data one can look at the original publication. For the galaxy M33, each region shows its own accurate coordinates. For the other galaxies, we published the X,Y coordinates starting from the centre of the galaxy. So, for these galaxies, one will find only the same coordinates of the center of the galaxy for all HII regions. J_A+AS_131_319.xml Comprehensive tables for the interpretation and modeling of the light curves of eclipsing binaries J/A+AS/131/395 J/A+AS/131/395 Eclipsing binaries light curves models Comprehensive tables for the interpretation and modeling of the light curves of eclipsing binaries A Claret Astron. Astrophys. Suppl. Ser. 131 395 1998 1998A&AS..131..395C J/A+AS/109/441 : Stellar models until He burning - I. (Claret, 1995) J/A+AS/114/549 : Stellar models until He burning - II. (Claret+, 1995) J/A+AS/125/439 : Stellar models until He burning - III. (Claret+, 1997) J/A+AS/110/329 : LTE model atmospheres coeff. (Diaz-cordoves+, 1995) J/A+AS/114/247 : Limb-darkening coefficients for RIJHK (Claret+, 1995) J/A+A/335/647 : Limb-darkening coefficients for ubvyUBVRIJHK (Claret 1998) Binaries, eclipsing Models, evolutionary binaries: eclipsing stars: evolution stars: fundamental parameters stars: interiors The results of the models are available, either as the set of 24 tables (table01 to table24) corresponding to the 24 different initial mass and composition, or as the set of tabulated parameters as a function of model and age. In the set of 24 tables, the parameters are described as sets of 7 lines, containing respectively: 1: Parameters from the model, as detailed in the bytes 1-96 of the "Byte-by-byte Decription of file: models.dat" section 2: Linear limb-darkening coefficients, as detailed in the "Byte-by-byte Decription of file: ld1.dat" section 3-6: Quadratic limb-darkening coefficients, as detailed in the "Byte-by-byte Decription of file: ld2*.dat" section 7: Photometric parameters from the models, as in bytes 98-144 of the "Byte-by-byte Decription of file: models.dat" section In tables 1 to 24, the parameters are described as follow: ------------------------------------------------------------------------------ Line one: ------------------------------------------------------------------------------ 1- 5 I5 -- N Number of the model in the track 6- 18 D12.6 yr Age Age of models 19- 26 F8.4 [solLum] log(L) Total luminosity 27- 34 F8.4 [cm/s2] log(g) Surface gravity 35- 42 F8.4 [K] log(Teff) Effective temperature 43- 50 F6.4 [solMass] Mass Mass of the model 51- 57 F6.3 --- log(k2) Apsidal motion constant (j=2) 58- 64 F6.3 --- log(k3) Apsidal motion constant (j=3) 65- 71 F6.3 --- log(k4) Apsidal motion constant (j=4) 72- 80 D8.3 --- alpha alpha = -Ep x R/GM^2 81- 87 F6.3 ---- beta Fractional gyration radius 88- 96 F6.4 ---- beta_1 Gravity-Darkening exponent ------------------------------------------------------------------------------ Line two: ------------------------------------------------------------------------------ 1- 8 F8.4 --- u(u) Linear Limb-darkening coef. (Stroemgren u) 9- 16 F8.4 --- u(v) Linear Limb-darkening coef. (Stroemgren v) 17- 24 F8.4 --- u(b) Linear Limb-darkening coef. (Stroemgren b) 25- 32 F8.4 --- u(y) Linear Limb-darkening coef. (Stroemgren y) 33- 40 F8.4 --- u(U) Linear Limb-darkening coef. (Johnson U) 41- 48 F8.4 --- u(B) Linear Limb-darkening coef. (Johnson B) 49- 56 F8.4 --- u(V) Linear Limb-darkening coef. (Johnson V) 57- 64 F8.4 --- u(R) Linear Limb-darkening coef. (R) 65- 72 F8.4 --- u(I) Linear Limb-darkening coef. (I) 73- 80 F8.4 --- u(J) Linear Limb-darkening coef. (J) 81- 88 F8.4 --- u(H) Linear Limb-darkening coef. (H) 89 96 F8.4 --- u(K) Linear Limb-darkening coef. (K) ------------------------------------------------------------------------------ Line three: ------------------------------------------------------------------------------ 1- 8 F8.4 --- a(u) Quadratic Limb-darkening coef. (Stroemgren u) 9- 16 F8.4 --- a(v) Quadratic Limb-darkening coef. (Stroemgren v) 17- 24 F8.4 --- a(b) Quadratic Limb-darkening coef. (Stroemgren b) 25- 32 F8.4 --- a(y) Quadratic Limb-darkening coef. (Stroemgren y) 33- 40 F8.4 --- a(U) Quadratic Limb-darkening coef. (Johnson U) 41- 48 F8.4 --- a(B) Quadratic Limb-darkening coef. (Johnson B) 49- 56 F8.4 --- a(V) Quadratic Limb-darkening coef. (Johnson V) 57- 64 F8.4 --- a(R) Quadratic Limb-darkening coef. (R) 65- 72 F8.4 --- a(I) Quadratic Limb-darkening coef. (I) 73- 80 F8.4 --- a(J) Quadratic Limb-darkening coef. (J) 81- 88 F8.4 --- a(H) Quadratic Limb-darkening coef. (H) 89 96 F8.4 --- a(K) Quadratic Limb-darkening coef. (K) ------------------------------------------------------------------------------ Line four: ------------------------------------------------------------------------------ 1- 8 F8.4 --- b(u) Quadratic Limb-darkening coef. (Stroemgren u) 9- 16 F8.4 --- b(v) Quadratic Limb-darkening coef. (Stroemgren v) 17- 24 F8.4 --- b(b) Quadratic Limb-darkening coef. (Stroemgren b) 25- 32 F8.4 --- b(y) Quadratic Limb-darkening coef. (Stroemgren y) 33- 40 F8.4 --- b(U) Quadratic Limb-darkening coef. (Johnson U) 41- 48 F8.4 --- b(B) Quadratic Limb-darkening coef. (Johnson B) 49- 56 F8.4 --- b(V) Quadratic Limb-darkening coef. (Johnson V) 57- 64 F8.4 --- b(R) Quadratic Limb-darkening coef. (R) 65- 72 F8.4 --- b(I) Quadratic Limb-darkening coef. (I) 73- 80 F8.4 --- b(J) Quadratic Limb-darkening coef. (J) 81- 88 F8.4 --- b(H) Quadratic Limb-darkening coef. (H) 89 96 F8.4 --- b(K) Quadratic Limb-darkening coef. (K) ------------------------------------------------------------------------------ Line five: ------------------------------------------------------------------------------ 1- 8 F8.4 --- c(u) Square root Limb-darkening coef. (Stroemgren u) 9- 16 F8.4 --- c(v) Square root Limb-darkening coef. (Stroemgren v) 17- 24 F8.4 --- c(b) Square root Limb-darkening coef. (Stroemgren b) 25- 32 F8.4 --- c(y) Square root Limb-darkening coef. (Stroemgren y) 33- 40 F8.4 --- c(U) Square root Limb-darkening coef. (Johnson U) 41- 48 F8.4 --- c(B) Square root Limb-darkening coef. (Johnson B) 49- 56 F8.4 --- c(V) Square root Limb-darkening coef. (Johnson V) 57- 64 F8.4 --- c(R) Square root Limb-darkening coef. (R) 65- 72 F8.4 --- c(I) Square root Limb-darkening coef. (I) 73- 80 F8.4 --- c(J) Square root Limb-darkening coef. (J) 81- 88 F8.4 --- c(H) Square root Limb-darkening coef. (H) 89 96 F8.4 --- c(K) Square root Limb-darkening coef. (K) ------------------------------------------------------------------------------ Line six: ------------------------------------------------------------------------------ 1- 8 F8.4 --- d(u) Square root Limb-darkening coef. (Stroemgren u) 9- 16 F8.4 --- d(v) Square root Limb-darkening coef. (Stroemgren v) 17- 24 F8.4 --- d(b) Square root Limb-darkening coef. (Stroemgren b) 25- 32 F8.4 --- d(y) Square root Limb-darkening coef. (Stroemgren y) 33- 40 F8.4 --- d(U) Square root Limb-darkening coef. (Johnson U) 41- 48 F8.4 --- d(B) Square root Limb-darkening coef. (Johnson B) 49- 56 F8.4 --- d(V) Square root Limb-darkening coef. (Johnson V) 57- 64 F8.4 --- d(R) Square root Limb-darkening coef. (R) 65- 72 F8.4 --- d(I) Square root Limb-darkening coef. (I) 73- 80 F8.4 --- d(J) Square root Limb-darkening coef. (J) 81- 88 F8.4 --- d(H) Square root Limb-darkening coef. (H) 89 96 F8.4 --- d(K) Square root Limb-darkening coef. (K) ------------------------------------------------------------------------------ Line seven: ------------------------------------------------------------------------------ 1- 8 F8.4 --- M_v Absolute Visual Magnitude 9- 16 F8.4 --- M_bol Absolute Bolometric Magnitude 17- 24 F8.4 --- U-B Color Index U-B (Johnson) 25- 32 F8.4 --- B-V Color Index B-V (Johnson) 33- 40 F8.4 --- u-b Color Index u-b (Stroemgren) 41- 48 F8.4 --- b-y Color Index b-y (Stroemgren) ------------------------------------------------------------------------------ We present parameters used in the investigation of the light curves of eclipsing binaries together with other data needed for the interpretation of their stellar and dynamical evolution. Parameters include limb-darkening coefficients and gravity darkening exponents, while data include the apsidal motion constants, the moment of inertia, and the potential energy. The adopted stellar models are those computed by Claret (1995, Cat. <J/A+AS/109/441>) for a representative chemical composition of X=0.70 and Z=0.02. In addition to the parameters needed for the study of the dynamical behavior and tidal evolution of binary systems, we supply the linear limb-darkening coefficients computed in 12 different photometric bands, as well as the gravity darkening exponent for each point along the evolutionary track. We have developed a method, based on the triangles strategy by Kippenhahn et al. 1967 to compute the gravity-darkening exponent using interior models. For the first time, the gravity-darkening exponents are presented as a function of mass and age. The old values of {beta}_1_ (0.32 and 1.0 for convective and radiative envelopes) are thus superseded by the present calculations and a smooth transition is achieved between both energy transport mechanisms. The tables presented here assist modeling of the light curves of close binaries using limb-darkening and gravity darkening coefficients which are consistent with the observed masses, radii and effective temperatures. In order to facilitate the use of the grid of models presented here in a variety of different research fields other than binary stars, synthetic colors (U-B, B-V, u-b, b-y) and M_v_ are also given.
Initial parameters Table Table number --- logM Initial mass [solMass] X X initial composition (H) --- Y Y initial composition --- Overshoot without (n) or with (y) overshooting --- Parameters from models Table Table number --- N Number of the model in the track -- Age Age of models yr log(L) Total luminosity [solLum] log(g) Surface gravity [cm/s2] log(Teff) Effective temperature [K] M Mass of the model solMass log(k2) Apsidal motion constant (j=2) --- log(k3) Apsidal motion constant (j=3) --- log(k4) Apsidal motion constant (j=4) --- alpha alpha = -Ep x R/GM^2^ --- beta Fractional gyration radius ---- beta_1 Gravity-Darkening exponent ---- Mvis Absolute visual magnitude mag Mbol Absolute bolometric magnitude mag U-B Color index U-B (Johnson) mag B-V Color index B-V (Johnson) mag u-b Color index u-b (Stroemgren) mag b-y Color index b-y (Stroemgren) mag Linear limb-darkening coeff. Table Table number --- N Number of the model in the track -- u(u) Linear Limb-darkening coeff. (Stroemgren u) --- u(v) Linear Limb-darkening coeff. (Stroemgren v) --- u(b) Linear Limb-darkening coeff. (Stroemgren b) --- u(y) Linear Limb-darkening coeff. (Stroemgren y) --- u(U) Linear Limb-darkening coeff. (Johnson U) --- u(B) Linear Limb-darkening coeff. (Johnson B) --- u(V) Linear Limb-darkening coeff. (Johnson V) --- u(R) Linear Limb-darkening coeff. (R) --- u(I) Linear Limb-darkening coeff. (I) --- u(J) Linear Limb-darkening coeff. (J) --- u(H) Linear Limb-darkening coeff. (H) --- u(K) Linear Limb-darkening coeff. (K) --- Quadratic limb-darkening coeff., a Quadratic limb-darkening coeff., b Square root limb-darkening coefficients, c Square root limb-darkening coefficients, d Table Table number --- N Number of the model in the track -- u Quadratic Limb-darkening coeff. (Stroemgren u) --- v Quadratic Limb-darkening coeff. (Stroemgren v) --- b Quadratic Limb-darkening coeff. (Stroemgren b) --- y Quadratic Limb-darkening coeff. (Stroemgren y) --- U Quadratic Limb-darkening coeff. (Johnson U) --- B Quadratic Limb-darkening coeff. (Johnson B) --- V Quadratic Limb-darkening coeff. (Johnson V) --- R Quadratic Limb-darkening coeff. (R) --- I Quadratic Limb-darkening coeff. (I) --- J Quadratic Limb-darkening coeff. (J) --- H Quadratic Limb-darkening coeff. (H) --- K Quadratic Limb-darkening coeff. (K) --- table01.txt logM= 0.0000 ,X=0.70, Z=0.02, without overshooting table02.txt logM= 0.0212 ,X=0.70, Z=0.02, without overshooting table03.txt logM= 0.0492 ,X=0.70, Z=0.02, without overshooting table04.txt logM= 0.0719 ,X=0.70, Z=0.02, without overshooting table05.txt logM= 0.0969 ,X=0.70, Z=0.02, with overshooting table06.txt logM= 0.1239 ,X=0.70, Z=0.02, with overshooting table07.txt logM= 0.1492 ,X=0.70, Z=0.02, with overshooting table08.txt logM= 0.1761 ,X=0.70, Z=0.02, with overshooting table09.txt logM= 0.1987 ,X=0.70, Z=0.02, with overshooting table10.txt logM= 0.2504 ,X=0.70, Z=0.02, with overshooting table11.txt logM= 0.2101 ,X=0.70, Z=0.02, with overshooting table12.txt logM= 0.3997 ,X=0.70, Z=0.02, with overshooting table13.txt logM= 0.4997 ,X=0.70, Z=0.02, with overshooting table14.txt logM= 0.5997 ,X=0.70, Z=0.02, with overshooting table15.txt logM= 0.6998 ,X=0.70, Z=0.02, with overshooting table16.txt logM= 0.8000 ,X=0.70, Z=0.02, with overshooting table17.txt logM= 0.8998 ,X=0.70, Z=0.02, with overshooting table18.txt logM= 1.0000 ,X=0.70, Z=0.02, with overshooting table19.txt logM= 1.1089 ,X=0.70, Z=0.02, with overshooting table20.txt logM= 1.1998 ,X=0.70, Z=0.02, with overshooting table21.txt logM= 1.2999 ,X=0.70, Z=0.02, with overshooting table22.txt logM= 1.3998 ,X=0.70, Z=0.02, with overshooting table23.txt logM= 1.5000 ,X=0.70, Z=0.02, with overshooting table24.txt logM= 1.6000 ,X=0.70, Z=0.02, with overshooting Patricia Bauer CDS 1998 May 28 Antonio Claret <claret@iaa.es> J_A+AS_131_395.xml Polarimetry of southern peculiar early-type stars J/A+AS/131/401 J/A+AS/131/401 Southern peculiar early-type stars polarimetry Polarimetry of southern peculiar early-type stars R V Yudin A Evans Astron. Astrophys. Suppl. Ser. 131 401 1998 1998A&AS..131..401Y J/A+AS/104/315 : Member of Herbig Ae/Be stellar group (The+ 1994) Polarization Stars, early-type circumstellar matter polarization stars: emission-line, Be stars: pre-main sequence We present and discuss optical polarimetry of a large group (60 objects) of peculiar early-type stars (Herbig Ae/Be stars and candidate members, B[e] stars, extreme emission line objects etc.). Most were taken from ``A new catalogue of members and candidate members of Herbig Ae/Be stellar group'' The et al. (1994, Cat. <J/A+AS/104/315>). For 40 out of the 60 objects polarization was measured for the first time. On the basis of the data we draw conclusions about the circumstellar shell configuration and orientation for several objects. Polarimetric variability on different time-scales (minutes...hours...days) was investigated, as well as comparison with earlier measurements to investigate variability over longer time-scales. No circular polarization was detected to a 5{sigma} level in most of the investigated stars. Polarimetric data obtained here as well as data available from the literature were analyzed from the point of investigating the evolutionary status of the objects. The relationship between the polarimetric and photometric data was also investigated.
Star positions Name Star name --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Polarimetry Name Star name --- HJD Julian date of the middle of observation d Filt Filter used --- Tint Basic integration time for the corresponding filter s Nint Number of integrations from which the values were obtained --- Plin Linear polarisation % e_Plin rms uncertainty on Plin % PA Equatorial position angle deg e_PA rms uncertainty on PA (North through East) deg sigma1 Internal error in PA number=1 Internal error calculated from photon counting statistics deg U U Stokes parameter (x100) % Q Q Stokes parameter (x100) % Pcirc Circular polarization % e_Pcirc rms uncertainty on Pcirc % tab6-11.tex LaTeX version of tables 6 to 11 tab12-16.tex LaTeX version of tables 12 to 16 tab17-22.tex LaTeX version of tables 17 to 22 tab6-11.ps PostScript version of the tables (Part. 1) tab12-16.ps PostScript version of the tables (Part. 2) tab17-22.ps PostScript version of the tables (Part. 3) Patricia Bauer CDS 1998 Apr 06 Ruslan Yudin <ruslan@pulkovo.spb.su> J_A+AS_131_401.xml A catalogue of accurate wavelengths in the optical spectrum of the Sun J/A+AS/131/431 J/A+AS/131/431 Accurate wavelengths in the Sun spectrum A catalogue of accurate wavelengths in the optical spectrum of the Sun C Allende Prieto R J Garcia Lopez Astron. Astrophys. Suppl. Ser. 131 431 1998 1998A&AS..131..431A Spectroscopy Sun catalogs line: identification Sun: photosphere techniques: spectroscopic Central line wavelengths in the spectrum of the Sun observed at the centre of the disc, and in the flux spectrum, line identification and solar log(gf).
Catalogue lambdaD Central wavelength in the disc-centre spectrum 0.1nm e_lambdaD Std. deviation from the 4-th order polyn. fit 0.1nm lambdaF Central wavelength in the flux spectrum 0.1nm e_lambdaF Std. deviation from the 4-th order polyn. fit 0.1nm Ion Chemical element and ionization state --- EP Excitation potential number=1 From Thevenin, 1989A&AS...77..137T and 1990A&AS...82..179T eV loggf Transition probabilities number=1 From Thevenin, 1989A&AS...77..137T and 1990A&AS...82..179T --- C. Allende Prieto Instituto de Astrofisica de Canarias 1998 Mar 23 C. Allende Prieto <callende@ll.iac.es> J_A+AS_131_431.xml B[e] stars. VI. MWC 297 = IRAS 18250-0351 J/A+AS/131/479 J/A+AS/131/479 Spectroscopy of MWC 297 B[e] stars. VI. MWC 297 = IRAS 18250-0351 Y Andrillat C Jaschek Astron. Astrophys. Suppl. Ser. 131 479 1998 1998A&AS..131..479A J/A+AS/117/281 : Spectroscopy of HD 51585 (= OY Gem) (Jaschek+, 1996) J/A+AS/118/495 : Spectroscopy of MWC 349 A (Andrillat+ 1996) J/A+AS/120/99 : Spectroscopy of MWC 645 (Jaschek+, 1996) J/A+AS/124/441 : Spectroscopy of HD 45677 = MWC 142 (Andrillat+ 1997) J/A+AS/128/475 : Spectroscopy of MWC 158 (Jaschek+ 1998) Equivalent widths Spectra, infrared Stars, emission Stars, early-type stars: emission-line, Be stars: individual (MWC 297, IRAS 18250-0351) stars: peculiar stars: variables: general On the basis of spectroscopic CCD material obtained at the Haute Provence Observatory, we provide line identifications and equivalent width measurements in the wavelength region 4100-8900{AA} of the spectrum of MWC 297. About two hundred features are identified, almost exclusively emission lines. Only one interstellar feature could be identified ({lambda}6613) a fact which contrasts with the eigth magnitudes of extinction found by photometrists. The spectrum of the underlying star corresponds probably to a late O or early B-type object. The cooler emission lines correspond to a spectrum of a middle A-type star. Analogies with other stars observed in this series of papers are examined.
MWC 297 IRAS 18250-0351 NZ Ser 18 27 39.5 -03 49 52
Equivalent widths and line identifications in the spectra of MWC 297 LambdaMea Measured wavelength 0.1nm Line Emission (e) or absorption (a) line --- EW Equivalent width 0.1nm n_EW Note on EW number=1 +f: refers to the following line w: wide --- LambdaLab Laboratory wavelength 0.1nm DLambda Measured minus laboratory wavelength 0.1nm Ident Line Identification and comments number=2 bl: blend Prob: probability Coinc: coincident --- Patricia Bauer CDS 1998 Jun 16 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_131_479.xml Atomic data from the IRON Project. XXIX. Radiative rates for transitions within the n=2 complex in ions of the boron isoelectronic sequence J/A+AS/131/499 J/A+AS/131/499 IRON Project XXIX. Boron isoelectronic sequence Atomic data from the IRON Project. XXIX. Radiative rates for transitions within the n=2 complex in ions of the boron isoelectronic sequence M E Galavis C Mendoza C J Zeippen Astron. Astrophys. Suppl. Ser. 131 499 1998 1998A&AS..131..499G J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions J/A+AS/123/159 : IRON Project XXII. C and O radiative rates J/A+AS/123/575 : IRON Project XXIII. Fe XXII excitation rate coefficients J/A+AS/126/373 : IRON Project XXVII. Fe IV collision strengths J/A+AS/131/153 : IRON Project XXXI. Fe XII electron excitation 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths 1997A&AS..122..167B : IRON Project XX. Fe I oscillator strengths 1997A&AS..122..177P : IRON Project XXI. Fe I fine-structure transition 1997A&AS..126..105B : IRON Project XXIV. Fe XXIV electron excitation 1998A&AS..127..545B : IRON Project XXV. Fe XII electron excitation 1997A&AS..126..365B : IRON Project XXVI. Fe IV oscillator strengths 1998A&AS..129..161B : IRON Project XXVIII. F-like ions fine-structure trans. Atomic physics atomic data atomic processes As part of the IRON Project, radiative rates have been calculated for the E1, E2 and M1 transitions within the n=2 complex in ions of the boron isoelectronic sequence (6<=Z<=28). The computations have been carried out with the atomic structure code SUPERSTRUCTURE which facilitates the generation of extended radiative datasets including configuration interaction, Breit-Pauli relativistic contributions and semi-empirical term-energy corrections. By means of extensive comparisons with the available datasets for this sequence, with detailed single-ion calculations and recent experiments, we have been able to assign accuracy ratings to the present A-values. We find that in general the spin-allowed and spin-forbidden E1 transitions are accurate to 10% and 20%, respectively, except for a few transitions in ions with Z<=7 that are perturbed by admixture with low-lying n=3 states (e.g. 2s^2^3l) and for those affected by the avoided crossing of the 2s2p^2^ ^2^S1/2 and ^2^P1/2 which takes place at Z~22. It is concluded that, statistically, the present dataset is the most accurate to date for this astrophysically relevant sequence.
Transition probabilities for ions with Z=6 to Z=28 Z Atomic number --- Ion Ion --- j j level --- i i level --- Aij Transition probability s-1 Patricia Bauer CDS 1998 Aug 13 Martha Elena Galavis <mgalavis@pion.ivic.ve> J_A+AS_131_499.xml Catalogue of HI maps of galaxies. I. J/A+AS/131/73 J/A+AS/131/73 Catalogue of HI maps of galaxies. I. Catalogue of HI maps of galaxies. I. M C Martin Astron. Astrophys. Suppl. Ser. 131 73 1998 1998A&AS..131...73M J/A+AS/131/77 : Catalogue of HI maps of galaxies. II. (Martin 1998) Galaxies, radio Galaxy catalogs H I data catalogs galaxies: fundamental parameters galaxies: ISM radio lines: galaxies A catalogue is presented of galaxies having large-scale observations in the HI line. This catalogue collects from the literature the information that characterizes the observations in the 21-cm line and the way that these data were presented by means of maps, graphics and tables, for showing the distribution and kinematics of the gas. It contains furthermore a measure of the HI extension that is detected at the level of the maximum sensitivity reached in the observations. This catalogue is intended as a guide for references on the HI maps published in the literature from 1953 to 1995 and is the basis for the analysis of the data presented in Paper II (Cat. <J/A+AS/131/77>).
Optical parameters of the galaxies Note Note for galaxies number=1 When several consecutive galaxies have an asterisk (*) for the first byte, they are enclosed in a same structure of gas, and the HI parameters contained in file hidata.dat are for the group of galaxies as a whole --- Name Galaxy name. --- Names Alternative name of the galaxy --- nLEDA Presence in LEDA catalogue number=2 If symbol ~ is present, the galaxy was not found in LEDA catalogue. In these cases the coordinates were taken from the reference (see the text) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Dopt The corrected optical diameter Do, from LEDA arcmin Type Morphological description number=3 S = Spiral E = Eliptical L = Lenticular I = Irregular C = Compact B = Bar R = Ring M = Multiple, possible interaction D = Dwarf --- MType Morphological Type Code (-6 to 10) --- HI parameters of the galaxies Note Note for galaxies number=1 When several consecutive galaxies have an asterisk (*) for the first byte, they are enclosed in a same structure of gas, and the HI parameters contained in file hidata.dat are for the group of galaxies as a whole --- Name Galaxy name --- Tel Radiotelescope used in the observation number=2 6m: 6.4-m (21-ft) parabolic antenna, Australia 11m: 11-m (36-ft) parabolic antenna, Australia 18m: 18.3m (60-ft) radio Telescope of Harvard Observatory, Great Britain Dwing: 25-m (82-ft) telescope at Dwingeloo, The Netherlands DRAO: 25-m (82-ft) radio telescope of the Dominion Radio Astrophysical Observatory, Canada IAR: 30-m radio telescope of the Instituto Argentino de Radioastronoma, Argentina Parkes: 64-m (210-ft) radio telescope of Australian National Radio Astronomical Observatory at Parkes, New South Wales, Australia Mk I: 76-m (250-ft) Mk I radio telescope at Jodrell Bank, Great Britain Mk IA: 76-m (250-ft) Mk IA radio telescope at Jodrell Bank, Great Britain 80m: 80-m (260-ft) radio telescope of the Ohio State University, USA 91m: NRAO 91-meter (300-ft) telescope in Green Bank, West Virginia, USA Effelsb: 100m (330-ft) radio telescope at Effelsberg, Germany Nancay: 200-m (655-ft) Nancay transit radio telescope, France Arecibo: 305-m (1000-ft) radio telescope at Arecibo, Puerto Rico ATCA: Australia Telescope Compact Array, Australia HM-C: Two elements interferometer of Cambridge Half-Mile radio telescope, Great Britain MRAO: half-mile telescope at the Mullard Radio Astronomy Observatory, Cavendish Laboratory, Cambridge NRint: Three-element interferometer of the NRAO Green Bank, USA OVRO: two-element interferometer of the Owens Valley Radio Observatory, California, USA TEST: Two-element synthesis telescope: Parkes 64-m radio telescope and a movable 18-m antenna, Australia VLA: Very Large Array of the NRAO, USA WSRT: Westerbork Synthesis Radio Telescope, The Netherlands --- HPBW Spatial resolution of the maps: half power beam width or synthesized beam arcmin Vres Velocity resolution of the maps km/s rms r.m.s. noise (in mJy/beam or K, see x_rms) of the maps at the spatial and velocity resolutions quoted in previous columns --- x_rms When *, the r.m.s. noise is in mJy/beam, else in K % Type of maps --- Map1 +: Map of the distribution of the total HI emission --- Mar2 +: Channel maps --- Map3 +: Position-velocity maps --- Map4 +: Individual profiles --- Map5 +: Tables --- Map6 +: Rotation curve --- Map7 +: Radial velocity Field --- Map8 +: Distribution of HI emission along one axis of the galaxy (see the text) --- Map9 +: Global HI profile of the integrated HI emission --- l_nHI Limit flag on nHI --- nHI Sensitivity reached in the observation, expressed by the lowest value of n(HI), only for Int-type maps 10+19cm-2 l_HIExt Limit flag on HIExt --- HIExt The largest extension of HI measured at n(HI) level of the previous column arcmin Notes Notes detailed in file notes.dat --- l_MHI/D0 Limit flag on MHI/D0 --- MHI/D0 HI mass, as given in the reference and by integration of the HI maps number=3 This quantity was unaffected by distance effects, to be helpful in the comparison of the total gas emission collected by different telescopes. 10+6solMass/Mpc2 Ref Reference (in refs.dat file) --- Notes to hidata.dat NoteN Note number --- Ntot Total number of lines for the reference --- Nline Running line number in range [1,Ntot] --- Text Text of the note --- References Ref Reference number --- BibCode Simbad bibcode --- Aut Author names and complete reference --- Patricia Bauer CDS 1998 Mar 31 Maria Cristina Martin J_A+AS_131_73.xml Catalogue of HI maps of galaxies. II. Analysis of the data J/A+AS/131/77 J/A+AS/131/77 Catalogue of HI maps of galaxies. II. Catalogue of HI maps of galaxies. II. Analysis of the data M C Martin Astron. Astrophys. Suppl. Ser. 131 77 1998 1998A&AS..131...77M J/A+AS/131/73 : Catalogue of HI maps of galaxies. I. (Martin 1998) Galaxies, radio Galaxy catalogs H I data galaxies: ISM galaxies: structure radio lines: galaxies We use some of the maps of the catalogue presented in Paper I (Cat. <J/A+AS/131/73>) to provide some evidence for global conditions that must be fulfilled by the galaxies to have extended hydrogen. For this purpose, we tried to find possible connections between the HI gas extension and other properties of the galaxies (morphological type, surface brightness, gas density, etc.). With isophotal hydrogen diameters of a large sample, we could observe that optically smaller galaxies seem to have greater relative HI extensions. By means of the relation with the apparent HI surface density, we found an expression that should provide a rough estimate of the gas extension. With respect to the dependence on morphological type, we could not find any significant correlation either for the real HI surface density or the relative gas extension. Nevertheless, whereas for spiral and irregular galaxies the real HI surface density exhibits a broad range of values, the values are rather lower for elliptical and S0 galaxies.
General parameters Name Galaxy name --- Names Alternative name of the galaxy --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Do The corrected optical diameter Do, from LEDA arcmin Type Morphological description number=1 S = Spiral E = Eliptical L = Lenticular I = Irregular C = Compact B = Bar R = Ring M = Multiple, possible interaction D = Dwarf --- Mtype Morphological type code --- Incl Inclination deg Dist Distance (see text) Mpc n_Dist -: indicates an interval --- Dist2 Second distance when interval (see text) Mpc Dlin Linear diameter from corrected optical diameter Do and distance kpc n_Dlin -: indicates an interval --- Dlin2 Second linear diameter when interval kpc MHI HI mass 10+9solMass n_MHI -: indicates an interval --- MHI2 Second HI mass when interval 10+9solMass SDHIa Apparent HI surface density 10+21/cm2 SDHIr Real HI surface density 10+20/cm2 HI observations Name Galaxy name --- Tel Radiotelescope used in the observation --- HPBW Spatial resolution of the maps: half power beam width or synthesized beam arcmin DHI/Do Ratio between HI and optical isophotal diameters --- r_DHI/Do Reference (in refs.dat file) --- References Ref Reference number --- BibCode Simbad bibcode --- Text Author names and complete reference --- Patricia Bauer CDS 1998 Mar 31 Maria Cristina Martin J_A+AS_131_77.xml Determination of proper motions and membership of the open clusters NGC 1750 and NGC 1758. J/A+AS/131/89 J/A+AS/131/89 NGC 1750 + NGC 1758 proper motions Determination of proper motions and membership of the open clusters NGC 1750 and NGC 1758. K -P Tian J -L Zhao Zh -Y Shao P B Stetson Astron. Astrophys. Suppl. Ser. 131 89 1998 1998A&AS..131...89T J/A+A/333/471 : NGC 1750 + NGC 1758 UBVRI photometry (Galadi-Enriquez+ 1998) J/A+AS/131/239 : NGC 1750 + NGC 1758 BVR photometry (Galadi-Enriquez+ 1998) Clusters, open Proper motions astrometry open clusters and associations: individual (NGC 1750, NGC 1758) The kinematic state of the open clusters NGC 1750 and NGC 1758 has been studied using newly determined proper motions for 540 stars in a field of 1.5{deg}x1.5{deg} in the Taurus dark cloud region. The proper motions are obtained from the reduction of PDS measurements of 20 plates that span a total time interval of 68 years, resulting in an average proper motion accuracy of 0.67mas/yr. These proper motions are used to determine the membership probabilities of stars in the region by means of a new, improved method described in this paper. Of the 540 stars analyzed here, 332 are found to be probable members of NGC 1750, and 23 are probable members of NGC 1758. The core radii of NGC 1750 and NGC 1758 are determined to be 17.2' and 2.25' respectively.
Proper motions and membership probabilities of stars in the region of NGC 1750 and NGC 1758 TZS98 Sequential number --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec pmx Relative proper motion in x mas/yr pmy Relative proper motion in y mas/yr e_pmx rms uncertainty on pmx mas/yr e_pmy rms uncertainty on pmy mas/yr p1750 Probability that star belongs to NGC 1750 --- p1758 Probability that star belongs to NGC 1758 --- Pfield Probability that star belongs to the field --- Nplate Number of plate pairs used in the present study --- Patricia Bauer CDS 1998 Sep 01 Tian Kaiping <tkp@center.shao.ac.cn> J_A+AS_131_89.xml The kinematics of 867 galactic planetary nebulae J/A+AS/132/13 J/A+AS/132/13 Planetary nebulae radial velocities The kinematics of 867 galactic planetary nebulae S Durand A Acker A Zijlstra Astron. Astrophys. Suppl. Ser. 132 13 1998 1998A&AS..132...13D V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) Planetary nebulae Radial velocities catalogs Galaxy: kinematics and dynamics planetary nebulae: general We present a compilation of radial velocities for 867 galactic planetary nebulae (Table 2.ps [postscript format] and Table2.dat [ascii format]).
Radial velocities for 867 Planetary Nebulae (PNe) Name Usual name of PN -- GLON Galactic longitude deg GLAT Galactic latitude deg nPNG Multiplicity index on PNG name number=1 SB 44 and SB 45 having the same PN G number, SB 44 = PN G356.0-7.4A, SB 45 = PN G356.0-7.4B --- PK PK number -- HRV Adopted heliocentric radial velocity number=2 Final data are calculated by a weighted average (see the article for more explanations) km/s e_HRV Adopted velocity uncertainty number=2 Final data are calculated by a weighted average (see the article for more explanations) km/s table2.ps *Radial velocities for 867 Planetary Nebulae (PNe) the PS version includes also high-, medium- and low-resolution velocities, SECAT (<V/84>) and recent literature data. Sophie Durand Obs. Strasbourg 1998 Oct 23 UNKNOWN UNKNOWN * 09-Oct-1998: First version which included a few errors in PN cross-identifications. * 23-Oct-1998: Problems in cross-identifications fixed. J_A+AS_132_13.xml The ROSAT all-sky survey catalogue of optically bright main-sequence stars and subgiant stars J/A+AS/132/155 J/A+AS/132/155 Main-sequence and subgiants ROSAT data The ROSAT all-sky survey catalogue of optically bright main-sequence stars and subgiant stars M Huensch H H M M Schmitt W Voges Astron. Astrophys. Suppl. Ser. 132 155 1998 1998A&AS..132..155H IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) IX/11 : ROSAT PSPC Source Catalog (Voges+ 1994) J/A+AS/127/251 : Giants and supergiants ROSAT data (Huensch+ 1998) J/A+AS/135/319 : Late-type main-sequence stars ROSAT data (Huensch+ 1999) Stars, dwarfs Stars, giant X-ray sources catalogs stars: activity stars: coronae stars: late-type X-rays: stars We present X-ray data for all main-sequence and subgiant stars of spectral types A, F, G, and K and luminosity classes IV and V listed in the Bright Star Catalogue (Cat. <V/50>) that have been detected as X-ray sources in the ROSAT all-sky survey; In addition to count rates, source detection parameters, hardness ratios, and X-ray fluxes we also list X-ray luminosities derived from Hipparcos parallaxes.
ROSAT
RASS detections of BSC late-type main-sequence stars n_HRName Note on star number=1 *: objects that have been observed later on in the course of the so-called "survey repair". Their X-ray data have been aquired at different times than the mayor part of the survey. --- HRName Bright Star Catalogue (Cat. <V/50>) number --- HD Henry Draper Catalogue (Cat. <III/135>) number --- Name Star's name --- Vmag V magnitude mag B-V B-V colour index mag SpType MK spectral classification --- Dist Distance pc Binary Binarity flag number=2 S: Single VB: Visual binary SB: Spectroscopic binary B: Other binary --- ExpTime Effective exposure time s Count Mean PSPC count rate ct/s e_Count Error of PSPC count rate ct/s LEx Likelihood of existence --- Delta Offset between optical and X-ray position arcsec HR Hardness Ratio = (H-S)/(H+S) --- e_HR Error of Hardness Ratio --- FX Apparent X-ray flux (0.1-2.4 keV) 10-17W/m2 LX X-ray luminosity 10+20W table2.ps PostScript version of table2 table2.tex LaTeX version of table2 Patricia Bauer CDS 1998 Apr 22 Matthias Huensch <supas106@astrophysik.uni-kiel.de> J_A+AS_132_155.xml Newly discovered candidate weak-line T Tauri stars in the surrounding area of the Taurus-Auriga region J/A+AS/132/173 J/A+AS/132/173 New weak-line T Tauri stars in Taurus-Auriga Newly discovered candidate weak-line T Tauri stars in the surrounding area of the Taurus-Auriga region J Z Li J Y Hu Astron. Astrophys. Suppl. Ser. 132 173 1998 1998A&AS..132..173L IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) J/A+A/312/439 : New T Tauri stars in Taurus-Auriga (Wichmann+, 1996) J/A+A/297/391 : T Tauri stars ROSAT survey (Neuhaeuser+, 1995) Stars, pre-main sequence X-ray sources stars: formation stars: pre-main sequence surveys X-rays: stars We present results of an extensive search for weak-line T Tauri stars (WTTS) in the outskirts of the Taurus-Auriga molecular cloud on the basis of the ROSAT All-Sky Survey Bright Source Catalog (Cat. <IX/10>). Our surveyed region extends from 2h 40m to 5h 40m in right ascension and from 10deg to 40deg in declination, with the central part of Taurus-Auriga(4h<{alpha}<5h, 15deg<{delta}<34deg), accomplished by Wichmann et al. (1996, Cat. <J/A+A/312/439>), excluded. Within a sky coverage of about 10$^{3}$ square degrees, 219 X-ray sources fullfill the criteria for selecting program sources suggested by Neuhauser et al. (1995A&A...295L...5N) and 164 of these X-ray sources were found to have at least one optical counterpart with E magnitude brighter than 16. Low-resolution spectroscopic observation has been carried out in order to discard early type stars and galaxies from the sample, additional intermediate-resolution spectra of a sub-sample of 156 late type optical counterparts were obtained for spectral classification and for the calculation of the equivalent width of H{alpha} emission and LiI line absorption at 6707{AA}. Excluding 2 previously identified WTTS, a total of 75 new candidate WTTS and one possible classical T Tauri star have been discovered in our study. The majority of the newly found Li-rich optical counterparts are believed to b e PMS stars rather than ZAMS stars as those of the Pleiades.
Optical data of the newly discovered candidate WTTS Optical data of the possible CTTS discovered and the two previously found WTTS candidates Optical data of the probable cloud members of Taurus-Aurigae Optical data of the possible optical counterparts to the RASS sources No Number --- m_No Multiplicity index on No --- 1RXS RASS (Cat. <IX/10>) designation --- RAh Right Ascension for equinox 2000.0 h RAm Right Ascension for equinox 2000.0 min RAs Right Ascension for equinox 2000.0 s DE- Declination sign --- DEd Declination for equinox 2000.0 deg DEm Declination for equinox 2000.0 arcmin DEs Declination for equinox 2000.0 arcsec Vmag Visual magnitude of the optical counterpart mag n_Vmag ? for unknown value --- EW(Ha) Equivalent width for H{alpha} number=1 These data are not in table5.dat 0.1nm EW(LiI) Equivalent width for LiI absorption line number=1 These data are not in table5.dat 0.1nm SpType Spectral type number=2 >M0V represents spectral type later than M0V, and so forth. --- Name Catalog identifier --- Com comments on optical position --- tables.ps PostScript version of the tables tables.tex LaTeX version of the tables Patricia Bauer CDS 1998 Apr 24 Jinzeng LI <ljz@nova.bao.ac.cn> J_A+AS_132_173.xml A statistical study of the spectra of very luminous IRAS galaxies. II. Spectral and environmental analysis J/A+AS/132/181 J/A+AS/132/181 Very luminous IRAS galaxies spectra. II. A statistical study of the spectra of very luminous IRAS galaxies. II. Spectral and environmental analysis H Wu Z L Zou X Y Xia Z G Deng Astron. Astrophys. Suppl. Ser. 132 181 1998 1998A&AS..132..181W J/A+AS/127/521 : Very luminous IRAS galaxies spectra. I. (Wu+ 1998) Galaxies, spectra Infrared sources Spectroscopy galaxies: active galaxies: interactions galaxies: starburst infrared: galaxies Spectroscopic observations of a sample of 73 very luminous IRAS galaxies (log(L_IR_/L_{sun}_)>=11.5 for H_0_=50km/s/Mpc, q_0_=0.5) from the 2Jy redshift survey catalogue were carried out using the 2.16m telescope at the Beijing Astronomical Observatory. The observational data, including the optical images (extracted from Digital Sky Survey) and spectra for these galaxies, are presented in paper I (Wu et al., 1998, Cat. <J/A+AS/127/521>). In this paper, we give the spectral and morphological classifications for these very luminous IRAS galaxies (VLIRGs). We show that about 60% of VLIRGs exhibit AGN-like spectra (Seyfert 1s, Seyfert 2s, LINER-like galaxies). This fraction goes up to 82% for the ultraluminous IRAS galaxies (ULIRGs) subsample (Log(L_IR_/ L_{sun}_)>=12.0). 56% of the VLIRGs show strong interaction or merging signatures; this fraction rises to 91% for the ULIRGs. These statistical results strongly suggest that interaction triggers nuclear activities and enhances the infrared luminosity. We find that LINER and a mixture type which have optical properties of both HII galaxies and LINERs could be at the transition stage from infrared luminous HII galaxies to AGNs; their main energy production is from starbursts as well as AGNs. Both infrared luminosities and Ha equivalent widths increase dramatically as nuclear separations between VLIRGs and their nearest neighbors decrease. There is little doubt that strong starbursts happen in the nuclei of VLIRGs. Assuming class 0 as advanced merger, we construct a simple merger sequence, from morphological classes 1 to 4 (with near or far companions), to class 5 and 6 (interacting pairs and mergers) and then to class 0 (isolated galaxies). Along this sequence, VLIRGs evolve from HII galaxies to AGNs.
Reddenings, observed and dereddened line ratios and spectral classification n_IRAS Note on the source origin number=1 A bracket indicates the sources that not belong to the 73 complete sample --- IRAS Source name --- m_IRAS Companion galaxies --- E(B-V) Galactic extinction E(B-V) mag Ha/Hb Observed H{alpha} to H{beta} ratio --- u_Ha/Hb Uncertainty flag on Ha/Hb number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- E(B-V)o Color excess of VLIRGs from observed Ha/Hb mag u_E(B-V)o Uncertainty flag on E(B-V)o number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- log([OIII]/Hb) Logarithm of [OIII]5007/Hb --- u_log([OIII]/Hb) Uncertainty flag on log([OIII]/Hb) number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- log([OI]/Ha) Logarithm of [OI]6300/Ha --- u_log([OI]/Ha) Uncertainty flag on log([OI]/Ha) number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- log([NII]/Ha) Logarithm of [NII]6584/Ha --- u_log([NII]/Ha) Uncertainty flag on log([NII]/Ha) number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- log([SII]/Ha) Logarithm of [SII]6716+6731/Ha --- u_log([SII]/Ha) Uncertainty flag on log([SII]/Ha) number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- 6563/4861 Continuum color ratio at 6563A and 4861A --- u_6563/4861 Uncertainty flag on 6563/4861 number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- SpType Spectral types number=3 S1: Seyfert 1 S2: Seyfert 2 L: LINER H: HII galaxy LH: mixture type with properties of both LINER and HII galaxy S?: Seyfert 2 or LINER --- Class Classification in Verons Catalog (1993, Cat. <VII/166>) number=4 Classification in Verons (1993, Cat. <VII/166>): S1: Seyfert 1 S2: Seyfert 2 H2: HII galaxy S or S?: Could be Seyfert or LINER. --- Ha/Hbth Theoretical Ha and Hb ratio --- log([OIII]/Hb)0 Logarithm of dereddened [OIII]5007/Hb --- u_log([OIII]/Hb)0 Uncertainty flag on log([OIII]/Hb)0 number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- log([OI]/Ha)0 Logarithm of dereddened [OI]6300/Ha --- u_log([OI]/Ha)0 Uncertainty flag on log([OI]/Ha)0 number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- log([NII]/Ha)0 Logarithm of dereddened [NII]6584/Ha --- u_log([NII]/Ha)0 Uncertainty flag on log([NII]/Ha)0 number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- log([SII]/Ha)0 Logarithm of dereddened [SII]6716+6731/Ha --- u_log([SII]/Ha)0 Uncertainty flag on log([SII]/Ha)0 number=2 The uncertainty is about 15%. (:): mean uncertainties 30% (;): mean uncertainties 50% --- Environmental and morphological parameters n_IRAS Note on source origin number=1 A bracket indicates the sources that not belong to the 73 complete sample --- IRAS Source name --- m_IRAS Companion galaxies --- Dist Distance of VLIRGs (H_0_=50km/s/Mpc,q_0_=0.5) Mpc MType Morphological types number=2 Morphological classification (Lawrence et al., 1989MNRAS.240..329L) 0: isolated 1: distant faint companion 2: distant bright companion 3: near faint companion 4: near bright companion 5: interacting pair 6: merger or highly peculiar --- Sep Projected separation between the nearest companions kpc Dz Redshift difference of the nearest companion --- --- Comments --- tables.tex LaTeX version of the tables tables.ps PostSript version of the tables Patricia Bauer CDS 1998 Apr 03 Hong Wu <wu@bac.pku.edu.cn> J_A+AS_132_181.xml Observations of the Sun with the astrolabe of Santiago: 1995-1997 J/A+AS/132/195 J/A+AS/132/195 Astrolabe observations of the Sun in 1995-1997 Observations of the Sun with the astrolabe of Santiago: 1995-1997 F Noel Astron. Astrophys. Suppl. Ser. 132 195 1998 1998A&AS..132..195N J/A+AS/102/11 : Astrolabe observations of the Sun in 1990-1992 (Noel 1993) J/A+AS/106/327 : Observations of the Sun during 1993 at Santiago (Noel 1994) J/A+AS/106/441 : Second catalogue of Santiago (Noel, 1994) J/A+AS/113/131 : Observations of the Sun during 1994 (Noel, 1995) Positional data Sun astrometry Sun: general Observations of the Sun with a modified Danjon astrolabe at 30{deg} and 60{deg} zenith distances have been carried out since 1990 at Santiago, Chile. Here are presented the results in right ascension, parameter Y and apparent semidiameter obtained during the period 1995-1997. These results and those obtained in for mer years are available in electronic form. The differences astrolabe minus ephemeris in {alpha} and semidiameter are briefly discussed.
Sun observations at 30{deg} zenith distance Sun observations at 60{deg} zenith distance Date Observation date "DD/MM/YY" MJD Modified Julian day d Zeu Zenith distance residual east upper border arcsec Zel Zenith distance residual east lower border arcsec Zwl Zenith distance residual west lower border arcsec Zwu Zenith distance residual west upper border arcsec dRA Right ascension (observed-ephemeris) s e_dRA rms uncertainty on dAlpha s Y Zenith distance (Observed-Adopted) + Declination(O-C) cos S. arcsec dDSun Sun semi-diameter (O-C) arcsec e_dDSun Sigma of dDSun and Y arcsec DSun Observed Sun semi-diameter reduced to AU. arcsec Patricia Bauer CDS 1998 May 05 Fernando Noel <fnoel@das.uchile.cl> J_A+AS_132_195.xml A survey of SiO emission towards interstellar masers. I. SiO line characteristics. J/A+AS/132/211 J/A+AS/132/211 SiO masers A survey of SiO emission towards interstellar masers. I. SiO line characteristics. J Harju K Lehtinen R S Booth I Zinchenko Astron. Astrophys. Suppl. Ser. 132 211 1998 1998A&AS..132..211H Infrared sources Masers Spectra, infrared ISM: clouds ISM: jets ISM: molecules radio lines: ISM stars: formation The results of a survey of SiO emission using the 15-m SEST and the 20-m Onsala telescope are presented in two tables. The sample contains altogether 369 objects including 270 H2O masers, 19 OH masers and 62 IRAS sources with colours typical for ultracompact HII regions. The remaining target sources consist of dust continuum peaks a CS emission peak near H2O masers (12) and Herbig-Haro objects (6). The entries are arranged according to increasing right ascension.
Observed SiO J=2-1 line parameters, SEST Observed SiO J=3-2 line parameters, SEST Observed SiO J=2-1 line parameters, Onsala Source Source number --- Name Source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Dist Distance kpc r_Dist Distance reference number=1 When no reference is given the distance is a kinematic distance calculated from the cloud velocity by using the galactic rotation curve determined by Brand & Blitz (1993, Cat. <J/A+A/275/67>) for R_0_=8.5kpc and {theta}_0_=220km/s. For sources in the first and fourth quadrants with a distance ambiguity the near kinematic distance was assumed. When no value is given when no solution has been found with the kinematical model, nor any reference to a photometric distance. Distance references: a: Jenniskens & Wouterloot (1990A&A...227..553J) b: Brand & Blitz (1993, Cat. <J/A+A/275/67) c: Avedisova & Palous (1989BAICz..40...42A) d: Henning et al. (1990A&A...227..542H) e: Simpson & Rubin (1990ApJ...354..165S) f: Cernicharo et al. (1985A&A...149..273C) g: Braz et al. (1990A&A...236..479B) h: Clemens & Barvainis (1988ApJS...68..257C) i: Genzel & Downes (1977A&AS...30..145G) --- Line SiO line (2-->1 or 3-->2) --- FigFile Name of the figure with the spectrum in subdirectory fig --- TA* Peak antenna temperature of the SiO line K e_TA* rms uncertainty on TA* K Vpeak Peak velocity km/s Vmin Minimum velocity km/s Vmax Maximum velocity km/s Vcen Centroid velocity (=(V_min + V_max)/2) km/s Vmean Intensity weighted average velocity km/s e_Vmean rms uncertainty on Vmean km/s FW Full width of the detected SiO line number=2 FW = V_max - V_min km/s Width SiO line width (variance or the second moment) km/s e_Width rms uncertainty on Width km/s Area Integrated intensity of the SiO line K.km/s e_Area rms uncertainty on Area K.km/s P Asymmetry parameter of the SiO line number=3 P = 2*(V_peak - V_cen)/FW --- Rem Remarks number=4 References to other surveys and association with a known object within 20 arcseconds. A reference is given without brackets if the positional coincidence is better than 5 arcseconds, and in brackets if the difference between the used coordinates is 5-20 arcseconds. A: Anglada et al. (1996ApJ...463..205A) Arc: Comoretto et al. (1990A&AS...84..179C), Palagi et al. (1993, Cat. <J/A+AS/101/153>) Brand et al. (1994, Cat. <J/A+AS/103/541>) B&E: Braz & Epchtein (1983A&AS...54..167B) B89: Braz et al. (1989A&AS...77..465B) B90: Braz et al. (1990A&A...236..479B) Bro: Bronfman et al. (1996, , Cat. <J/A+AS/115/81>) C: Churchwell et al. (1990A&AS...83..119C) Cha: Chan et al. (1996, Cat. <J/A+AS/115/285>) C95: Caswell et al. (1995MNRAS.277..210C) C96: Caswell (1996MNRAS.279...79C) CV95: Caswell & Vaile (1995MNRAS.273..328C) E: Ellingsen et al. (1996MNRAS.280..378E) G: Gaume & Mutel (1987ApJS...65..193G) Gen: Gensheimer et al. (1996A&A...314..281G) H: Henning et al. (1992A&AS...93..525H) Has: Haschick et al. (1983ApJ...265..281H) Hof: Hofner & Churchwell (1996, Cat. <J/A+AS/120/283>) J: Jenness et al. (1995MNRAS.276.1024J) Juv: Juvela (1996, Cat. <J/A+AS/118/191>) M: Molinari et al. (1996, Cat. <J/A+A/308/573>) Mor: Moreira et al. (1995ApJ...454..850M) Men: Menten (1991ApJ...380L..75M) P: Plume et al. (1992ApJS...78..505P) Sca: Scalise et al. (1989A&A...221..105S) vdW: van der Walt et al. (1995, Cat. <J/A+AS/110/81>) WB: Wouterloot & Brand (1989, Cat. <J/A+AS/80/149>) W&W: Wouterloot & Walmsley (1986A&A...168..237W) Z94: Zinchenko et al. (1994, Cat. <J/A+A/288/601>) Z95: Zinchenko et al. (1995, Cat. <J/A+AS/111/95>) --- SEST source catalogue Onsala source catalogue Source Source number --- Name Source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Dist Distance kpc r_Dist Distance reference number=1 When no reference is given the distance is a kinematic distance calculated from the cloud velocity by using the galactic rotation curve determined by Brand & Blitz (1993, Cat. <J/A+A/275/67>) for R_0_=8.5kpc and {theta}_0_=220km/s. For sources in the first and fourth quadrants with a distance ambiguity the near kinematic distance was assumed. When no value is given when no solution has been found with the kinematical model, nor any reference to a photometric distance. Distance references: a: Jenniskens & Wouterloot (1990A&A...227..553J) b: Brand & Blitz (1993, Cat. <J/A+A/275/67) c: Avedisova & Palous (1989BAICz..40...42A) d: Henning et al. (1990A&A...227..542H) e: Simpson & Rubin (1990ApJ...354..165S) f: Cernicharo et al. (1985A&A...149..273C) g: Braz et al. (1990A&A...236..479B) h: Clemens & Barvainis (1988ApJS...68..257C) i: Genzel & Downes (1977A&AS...30..145G) --- Cat Catalogue designation --- Fpeak Maximun flux density of the H2O maser number=2 H_2_O maser or sometimes OH maser, in which case clearly indicated Jy e_Fpeak rms uncertainty on Fpeak Jy Vmaser Velocity of the strongest maser component km/s Vmin Minimum velocity km/s Vmax Maximum velocity km/s Vcen Centroid velocity ((=(V_min + V_max)/2) km/s Vmean Intensity weighted average velocity km/s FW Full width of the maser emission feature number=3 FW = V_max - V_min km/s S Integrated flux density of the maser line Jy.km/s Vcloud Velocity of the associated molecular cloud km/s r_Vcloud [1/21] Cloud velocity reference number=4 The cloud velocity refers usually to the velocity of the associated dense core as estimated from CS data. When the latter has not been available, a radial velocity determined from NH3 or CO observations has been used. If no molecular line measurements has been found in the literature we have used for the kinematic distance estimate the peak radial velocity of the SiO(J=2-1) line from the present survey or the peak velocity of the associated maser. In this case, there is no velocity cloud data. Cloud velocity references: 1: Bronfman et al. (1996, Cat. <J/A+AS/115/81>) 2: Plume et al. (1992ApJS...78..505P) 3: Molinari et al. (1996, cat. <J/A+A/308/573>) 4: Anglada et al. (1996ApJ...463..205A) 5: Zinchenko et al. (1995, Cat. <J/A+AS/111/95>) 6: Juvela (1996, Cat. <J/A+AS/118/191>) 7: Wouterloot & Brand (1989, Cat. <J/A+AS/80/149>) 8: Churchwell et al. (1990A&AS...83..119C) 9: Jenness et al. (1995MNRAS.276.1024J) 10: Wouterloot et al. (1988A&A...203..367W) 11: Brand & Blitz (1993, Cat. <J/A+A/275/67>) 12: Fich et al. (1989ApJ...342..272F) 13: Lada et al. (1991ApJ...368..432L) 14: Haschick et al. (ApJ...265..281H) 15: Gardner & Whiteoak (1978MNRAS.183..711G) 16: Codella & Felli (1995A&A...302..521C) 17: Cesaroni et al. (1991A&A...252..278C) 18: Joncas et al. (1992ApJ...387..591J) 19: Haschick et al. (1983ApJ...265..281H) 20: Clemens & Barvainis (1988ApJS...68..257C) 21: Zinchenko et al. (1994, Cat. <J/A+A/288/601>) --- Rem Remarks number=5 See Note (4) of the preceding description. --- tableb1.tex LaTeX version of SEST data tableb1.ps Postscript version of SEST data tableb2.tex LaTeX version of Onsala data tableb2.ps Postscript version of Onsala data Patricia Bauer CDS 1998 May 22 Jorma Sakari Harju <harju@obs20.astro.helsinki.fi> J_A+AS_132_211.xml Continuous declination system set up by observations of photoelectric astrolabe Mark I in Irkutsk. The first results of international cooperation between CSAO and VS NIIFTRI. J/A+AS/132/233 J/A+AS/132/233 PHA I observations Continuous declination system set up by observations of photoelectric astrolabe Mark I in Irkutsk. The first results of international cooperation between CSAO and VS NIIFTRI. J Xu D Li J Liu H Cheng Z Zhang S I Raschotin V A Emeliyanov V V Kaplenko V T Zalutsky Astron. Astrophys. Suppl. Ser. 132 233 1998 1998A&AS..132..233X I/149 : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) - Extension (Fricke+ 1991) Fundamental catalog Positional data astrolabe observations star catalog The Photoelectric Astrolabe Mark I (PHA I) has been revised with a new combined prism which could work as an almucantar with zenith distance of 45 degree, to measure continuous declinations at the latitude of Irkutsk, Russia ({phi}=52 degree). The PHA I has been working at the astronomical base of VS NIIFTRI in Irkutsk since Nov. 1995, based on an international cooperation agreement of near 4 years for star catalogue and EOP measurements. The first observing program was ended in June 1997, giving corrections in both right ascension and declination to 200 stars with no blind zone in declination determination, which most astrolabe catalogues in the world usually would have.
The first preliminary catalog of PHA I FK5 No. of FK5 star --- Vmag V magnitude mag SpType Spectral type --- RAh Right ascension at observational epoch (J2000) h RAm Right ascension at observational epoch (J2000) min RAs Right ascension at observational epoch (J2000) s DE- Declination sign --- DEd Declination at observational epoch (J2000) deg DEm Declination at observational epoch (J2000) arcmin DEs Declination at observational epoch (J2000) arcsec DRA DRA (observation - FK5) s e_RAs rms uncertainty on RA s ERA1 15*e_RA*cos(declination) arcsec DDE DDE (observation - FK5) arcsec e_DEs rms uncertainty on declination arcsec Ep-1900 mean epoch of observation (1900+) yr Flag 1--basic star, 2--catalogue star --- Patricia Bauer CDS 1998 Mar 31 Xu Jiayan J_A+AS_132_233.xml Measurements of double stars 1993.67-1998.13 J/A+AS/132/237 J/A+AS/132/237 Double stars measurements Measurements of double stars 1993.67-1998.13 A Alzner Astron. Astrophys. Suppl. Ser. 132 237 1998 1998A&AS..132..237A J/A+AS/132/253 : 9 visual double stars orbital elements (Alzner 1998) Binaries, orbits Stars, double and multiple astrometry binaries: visual 624 Micrometer Measurements of 224 pairs with a 32.5 cm Cassegrain, 719 Measurements of 310 double stars with a 360 mm Newtonian are given.
624 Measurements of 224 double stars at the 32.5cm Cassegrain. 719 measures of 310 double stars with a 360mm Zeiss-Newtonian 1993.67-1996.50 ADS ADS number --- m_ADS Multiplicity index on ADS --- Name Star name --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin Obs Observation date yr PA Position angle deg n_Sep Note on PA and Sep number=1 r: round *: companion not seen s: single n: no companion seen e: elong. - not measured or dm not estimated ':': P.A. values are scattered, or P.A. or distance could not be measured accurately, mostly in case of faint pairs. --- Sep Separation angle arcsec u_Sep Uncertainty flag (:), or elongated (e) --- Nobs Number of observations --- dm Estimated brightness difference between the two stars of the pair mag n_dm2 Separation dash when interval --- dm2 Second value of dm when interval mag n_dm Note number=2 v: var qi: quadrant inverted --- Micr Micrometer type (in table1.dat) number=3 F: RETEL filar micrometer D: MECA PRECIS double image micrometer --- Residuals of 147 orbits from table1.dat Residuals of 106 orbits and notes from table3.dat Name ADS number or name --- m_Name Multiplicity index on ADS --- n_Name Note number=1 *: Because of the considerable dm the star is currently too difficult for the Cassegrain --- Ref References for the data (Authors, date) --- n_Ref Note on Ref number=2 a: the Elements given in the publication are wrong. --- theta (O-C) on PA deg rho (O-C) on Sep arcsec theta2 (O-C) on PA deg rho2 (O-C) on Sep arcsec theta3 (O-C) on PA deg rho3 (O-C) on Sep arcsec Note *: Individual note in table4.dat number=3 Individual notes: 17175 Hall 1949 : requires revision. also measured by CHARA and Heintz with the same tendency 2236 Heintz 1990 : probably measurement error 2755 Popovic & Pavlovic 1995: The rectilinear solution given by the same authors for this star is better. 5586 Baize : no other new measures are known 5958 Popovic 1982 : the orbit has to be revised 8884 Alzner 1996 : A longperiodic solution with P=450, T=1928, a=0.66, e=0.57, i=105, {omega}=53.5, node=9.6, favoured by the author, was sent to the Circular No.128 together with the shortperiodic one, but was not published there. Shortperiodic solutions seem to be ruled out now by Heintz' and Hipparcos' measurements, but also the P=450 orbit does not fit the Hipparcos distance 0.778" well. Any longperiodic orbit will stay undetermined for many years. No speckle measurements. 10230 Baize 1983 : The orbit has to be revised 11006 Heintz 1995 : starting retrograde motion? --- Patricia Bauer CDS 1998 May 05 A. Alzner J_A+AS_132_237.xml Orbital elements of 9 visual double stars J/A+AS/132/253 J/A+AS/132/253 9 visual double stars orbital elements Orbital elements of 9 visual double stars A Alzner Astron. Astrophys. Suppl. Ser. 132 253 1998 1998A&AS..132..253A J/A+AS/132/237 : Double stars measurements (Alzner 1998) Binaries, orbits Stars, double and multiple astrometry binaries: visual Orbital elements and ephemerides for 9 visual double stars are given.
General parameters Name Name --- Names Other name --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin Vmag1 Visual magnitude of the primary mag Vmag2 Visual magnitude of the secondary mag SpType Spectral type --- Plx Trigonometric parallax from Hipparcos mas Prec Precession factor for J2000 deg/yr P Period yr a Semi-major axis arcsec i Inclination deg W2000 Longitude of ascending node, J2000 deg T Time of perihelion passage yr e Ellipticity --- w Longitude of perihelion deg Pdyn Dynamical parallax mas MA+MB Total mass solMass Com Comments --- Bu 151 residuals: speckle measurements Bu 151 residuals: visual measurements Hu 39 residuals: low excentricity variant data Hu 39 residuals: high excentricity variant data STF 1130 residuals STF 2434 residuals STT 229 residuals STT 363 residuals STT 448 residuals STT 53 residuals STT 89 residuals Date Observation date yr n_Date In stt89.dat, 1896. for 1896-1898 --- PA Observed position angle deg n_PA Note on PA number=1 r: round *: perhaps elong. in P.A. 285 s: single ed: elongation doubtful --- Sep Observed separation arcsec n_Sep Note on Sep number=2 e: elong o: oval --- Nobs Number of observations --- --- --- Nobs2 Second number of observations --- n_Nobs m: many nights --- Obs Observators? --- theta (O-C) on PA deg rho (O-C) on Sep arcsec u_rho Uncertainty flag on the residuals --- Patricia Bauer CDS 1998 May 05 A. Alzner J_A+AS_132_253.xml Fifteen years monitoring of extragalactic radio sources at 22, 37 and 87GHz J/A+AS/132/305 J/A+AS/132/305 Extragal. radio sources at 22, 37 and 87GHz Fifteen years monitoring of extragalactic radio sources at 22, 37 and 87GHz H Terasranta M Tornikoski A Mujunen K Karlamaa T Valtonen N Henelius S Urpo M Lainela T Pursimo K Nilsson S Wiren A Lahteenmaki M Korpi R Rekola P Heinamaki M Hanski P Nurmi K Kokkonen P Keinanen O Joutsamo J Oksanen H Pietila E Valtaoja M Valtonen P Kononen Astron. Astrophys. Suppl. Ser. 132 305 1998 1998A&AS..132..305T J/A+AS/116/157 : SEST obs. of extragalactic radiosources (Tornikoski+, 1996) Galaxies, radio Radio sources BL Lacertae objects: general galaxies: active quasars: general radio continuum: galaxies radio continuum: general Over 13500 continuum observations of extragalactic sources are presented. These observations of 157 sources at 22, 37 and 87GHz more than doubles the millimeter observations of these sources. The data are between 1990.5 and 1995.5, and combined with our earlier published data form a 15 year database.
Source list with classification and number of observations at each frequency Object Object designation --- Name Other name --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Type Source Type number=1 HPQ: source that has been recorded at least once an optical polarization LPQ: source for which the polarization level has always been below 3.0% BLO: BL Lac object GAL: galaxy --- o_22GHz Number of observations at 22GHz --- o_37GHz Number of observations at 37GHz --- o_87GHz Number of observations at 87GHz --- Flux density data for 157 extragalactic radio sources observed with the Metsahovi-telescope at 22, 37 and 87GHz. Object Object designation --- Name Radiosource other name --- Freq Observing frequency (22, 37 or 87 GHz) GHz OBSdate Observation date "DD/MM/YY" OBSh Observation time (hours) h OBSm Observation time (minutes) min SFreq Flux density at frequency Jy e_SFreq 1 sigma error estimate of flux density Jy Patricia Bauer CDS 1998 Aug 25 Harri Terasranta <hte@cc.hut.fi> J_A+AS_132_305.xml Kinematical models for double radio sources and the unified scheme. II. The database J/A+AS/132/31 J/A+AS/132/31 Kinematical models for double radio sources Kinematical models for double radio sources and the unified scheme. II. The database K Nilsson Astron. Astrophys. Suppl. Ser. 132 31 1998 1998A&AS..132...31N VIII/15 : Parkes Radio Sources Catalogue (PKSCAT90) (Wright+ 1990) VIII/17 : The 1.4GHz Northern Sky Catalog (White+ 1992) VIII/16 : Molonglo Reference Catalogue of Radio Sources (Large+ 1991) VIII/4 : Fourth Cambridge Survey (4C) (Pilkington+ 1965; Gower+1967) VIII/43 : Radio survey of clusters of galaxies (Andernach+ 1978) VIII/13 : A new catalog of 53522 4.85GHz sources (Becker+ 1991) VII/2 : Master list of radio sources, updated 1978 (Dixon, 1970) VIII/5 : Bright Extragalactic Radio Sources (1Jy) (Kuehr+, 1981) VII/99 : Radial Velocities of Galaxies (Palumbo+ 1986) III/175 : Optical spectroscopy of radio sources (Stickel+, 1989-94) J/ApJS/81/83 : Compendium of Radio Spectra and Luminosities (Herbig+ 1992) Baryshev & Teerikorpi, Paper I. 1995A&A...295...11B Radio sources galaxies: active ISM: jets radio continuum: galaxies These tables contain structural parameters for a large sample of classical FR II (Fanaroff-Riley II, 1974MNRAS.167p..31F) double radio sources obtained from the literature.
Data for the HR (Herbig and Readhead, Cat. <J/ApJS/81/83>) and 2.5 Jy samples Data for sources not belonging to the HR and 2.5 Jy samples IAU IAU name of the source --- m_IAU Multiplicity index on IAU --- Name Other name of the source --- z Redshift of optical identification --- LAS Largest angular size of the radio structure arcsec SI Spectral index between 178MHz and 5GHz --- Sizel Projected linear size number=1 H_0_=50km/s/Mpc and q_0_=0.5 is assumed kpc logL Luminosity between 10MHz and 10GHz in the rest frame of the source number=1 H_0_=50km/s/Mpc and q_0_=0.5 is assumed [10-7W] S5GHZcore Flux of the core at 5 GHz mJy SIcore Spectral index of the core near 5 GHz --- Pc/Ptot Relative strength of the core at 5 GHz number=1 H_0_=50km/s/Mpc and q_0_=0.5 is assumed --- Q Arm length ratio number=2 Ratio fo the distances of the outermost hotspots at opposite sides from the radio core or the optical identification. Q>1 by definition --- D Bending angle deg F Lobe flux ratio number=3 F=S1/S2, where S1 is the flux density of the lobe farther from the core and S2 is the flux density of the lobe loser to the core --- nuF Frequency at which F has been measured MHz Flux% Interferometric flux/single dish flux number=4 Flux%=(Score+Slobes)/Stot, where Score is the flux density of the core, Slobes=S1+S2 is the flux density of the lobes and Stot is the total flux density of the source measured with a single dish radio telescope --- ID Optical identification number=5 'G': galaxy 'Q': Quasar ' ': unidentified --- Refmap Reference of the radio map (in refs.dat) --- n_Refmap Note on Refmap number=6 *: No actual radio map was available and the structural data was taken from tabular material --- Refs References in refs.dat file --- Sample Sample membership --- References Ref Reference number --- BibCode BibCode --- Aut Authors name --- Com Comments --- Patricia Bauer CDS 1998 May 15 Kari Nilsson <kani@deneb.astro.utu.fi> J_A+AS_132_31.xml Identification of selected sources for the ROSAT Galactic Plane Survey. I. J/A+AS/132/341 J/A+AS/132/341 ROSAT GPS optical identification Identification of selected sources for the ROSAT Galactic Plane Survey. I. C Motch P Guillout F Haberl J Krautter M W Pakull W Pietsh K Reinsch W Voges F -J Zickgraf Astron. Astrophys. Suppl. Ser. 132 341 1998 1998A&AS..132..341M IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) J/A+A/318/111 : ROSAT Galactic Plane Survey (Motch+ 1997) Cross identifications X-ray sources surveys X-rays: galaxies X-rays: general X-rays: stars We report on optical searches in the error circles of 93 ROSAT survey sources located at low galactic latitudes (|b|<20{deg}). These sources were extracted from the ROSAT Galactic Plane Survey using various selection criteria on hardness ratio, X-ray and optical brightness and integrated galactic absorption in the direction of the source. We find optical identifications in 76 cases, among which are 25 new AGN, 6 new CVs and a new Be/X-ray binary. In order to illustrate the relevance of the source selections applied here, we cross-correlated the ROSAT all-sky survey bright source list with SIMBAD. Different classes of X-ray emitters populate distinct regions of a multi dimensional parameter space involving flux ratios, galactic latitude and N_H_. This relatively good segregation offers the possibility to build source samples with enhanced probability of identification with a given class. Complete optical identification of such subsamples could eventually be used to compute meaningful probabilities of identification for all sources using as basis a restricted set of multi-wavelength information.
ROSAT
X-ray characteristics of ROSAT survey sources derived from the SASS as in October 1991 RXJ Source name --- Source Source selection origin number=1 X: X-ray binary like S: Soft white dwarf candidate A: Absorption supersoft candidate B: X-ray bright source O: Other remaining source --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec r90 90% confidence radius arcsec Count Count rate ct/s e_Count rms uncertainty on Count ct/s HR1 Hard ratio 1 --- e_HR1 rms uncertainty on HR1 --- HR2 Hard ratio 2 --- e_HR2 rms uncertainty on HR2 --- 1RXS 1RXS (Cat. <IX/10>) designation --- Optical identifications of ROSAT survey sources RXJ Source name --- Sel Source selection origin number=1 X: X-ray binary like S: Soft white dwarf candidate A: Absorption supersoft candidate B: X-ray bright source O: Other remaining source --- Dist X-ray to optical distance in units of the 90% confidence radius --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec IdOpt Optical identification --- Vmag V magnitude mag Bmag B magnitude mag Class Class number=2 AC: active corona Gal: Normal galaxy AGN: Active galactic nucleus Be/X: Be/X-ray binary UNID: Unidentified WD: Isolated white dwarf --- Mtype Spectral or morphological type --- Chart Y: a finding chart is provided --- Patricia Bauer CDS 1998 Oct 08 Christian Motch <motch@astro.u-strasbg.fr> J_A+AS_132_341.xml Optical observations of eight X-ray selected BL Lacertae objects J/A+AS/132/361 J/A+AS/132/361 Optical observations of eight BL Lacs Optical observations of eight X-ray selected BL Lacertae objects C M Raiteri M Villata G De Francesco L Lanteri M Cavallone G Sobrito Astron. Astrophys. Suppl. Ser. 132 361 1998 1998A&AS..132..361R J/A+AS/116/403 : RI photometry of stars in 12 BL Lac objects (Fiorucci+, 1996) BL Lac objects Magnitudes BL Lacertae objects: general galaxies: active Optical data in the Johnson's BV and Cousins' R bands are presented for eight X-ray selected BL Lacertae objects that have recently been pointed by the Satellite per Astronomia X `Beppo'(BeppoSAX). The observations were done with the 1.05m telescope of the Torino Astronomical Observatory and the observational periods include, or are close to, the satellite pointings. These data provide optical information on sources that have been rarely observed in the optical band. Moreover, they can be compared to the X-ray ones for a better understanding of the emission properties of these objects. Variability on short time scales (a few days) was found for MS 0317.0+1834, 1ES 0347-121, and MS 0737.9+7441. For a description of the (RI)c photometric system, see e.g. the General Catalog of Photometric Data <GCPD/54>
BVR observations BLLac Source designation --- HJD Heliocentric Julian date d Band Band --- mag Magnitude in the band Band mag e_mag rms uncertainty on mag mag Observations BLLac Source designation --- RAh Right ascension (2000.0) (from Simbad) h RAm Right ascension (2000.0) (from Simbad) min RAs Right ascension (2000.0) (from Simbad) s DE- Declination sign --- DEd Declination (2000.0) (from Simbad) deg DEm Declination (2000.0) (from Simbad) arcmin DEs Declination (2000.0) (from Simbad) arcsec Band Band --- Date1 Observation date (beginning) "DD/MM/YY" --- Separation dash --- Date2 Observation date (end) "DD/MM/YY" magmin Minimum magnitude mag magmax Maximum magnitude mag Nobs Number of observations --- C.M. Raiteri raiteri@to.astro.it Patricia Bauer CDS 1998 Aug 11 Claudia M. Raiteri <raiteri@to.astro.it> J_A+AS_132_361.xml Physical parameters of the Algol system TZ Eridani from simultaneous analysis of Geneva 7-colour light curves J/A+AS/132/367 J/A+AS/132/367 Geneva photometry of the Algol system TZ Eri Physical parameters of the Algol system TZ Eridani from simultaneous analysis of Geneva 7-colour light curves F Barblan P Bartholdi P North G Burki E C Olson Astron. Astrophys. Suppl. Ser. 132 367 1998 1998A&AS..132..367B II/169 : Catalogue of observations in the Geneva photometric system Binaries, eclipsing Photometry, Geneva binaries: eclipsing stars: fundamental parameters stars: individual (TZ Eri) Light curves of the semi-detached eclipsing binary system TZ Eridan in the Geneva 7-colour photometric system were analysed using the Wilson-Devinney programme. The physical and orbital parameters have been determined through a self-consistent simultaneous solution of the seven light curves and of the radial velocity curves of both components.
TZ Eri BD-06 880 04 21 40.2 -06 01 08
Photometry of TZ Eri HJD Heliocentric julian day d Q Photometric Q weight (Rufener, 1988, Cat. <II/169>) --- Vmag Magnitude in the visible mag P Photometric P weight (Rufener, 1988, Cat. <II/169>) --- [U-B] Geneva [U-B] index mag [V-B] Geneva [V-B] index mag [B1-B] Geneva [B1-B] index mag [B2-B] Geneva [B2-B] index mag [V1-B] Geneva [V1-B] index mag [G-B] Geneva [G-B] index mag Fz airmass --- Patricia Bauer CDS 1998 Apr 23 Pierre North <Pierre.North@obs.unige.ch> J_A+AS_132_367.xml The intraday variability in the radio-selected and X-ray-selected BL Lac objects J/A+AS/132/83 J/A+AS/132/83 BVRI photometry of 7 BL Lac objects The intraday variability in the radio-selected and X-ray-selected BL Lac objects J M Bai G Z Xie K H Li X Zhang W W Liu Astron. Astrophys. Suppl. Ser. 132 83 1998 1998A&AS..132...83B BL Lac objects Photometry, UBVRI BL Lacertae objects: general galaxies: photometry Seven BL Lac objects have been photometrically observed in an effort to study the difference of optical intraday variability between the radio-selected BL Lac objects (RBLs) and X-ray-selected BL Lac objects (XBLs). The objects we observed are selected arbitrarily. They are four RBLs, PKS 0735+178, PKS 0754+101, OJ 287 and BL Lac, and three XBLs, H 0323+022, H 0548-322 and H 2154-304. During the observation all of them exhibited microvariation, and H 0323+022 and H 0548-322 sometimes showed brightness oscillation. PKS 0735+178 and BL Lac were in their faint states and not very active. It seems that RBLs do not show microvariability more frequently than XBLs.
BL Lac 22 02 43.3 +42 16 40 H 0323+022 03 26 13.8 +02 25 15 H 0548-322 05 50 41.5 -32 16 09 H 2154-304 21 58 51.9 -30 13 30 OJ 287 PKS 0851+203 08 54 48.9 +20 06 31 PKS 0735+178 07 38 07.4 +17 42 19 PKS 0754+101 07 57 06.7 +09 56 35
Photometric data of seven BL Lac objects Date Observation date "DD/MM/YY" JD Julian Date d mag Magnitude mag e_mag One sigma uncertainty on mag mag Band Filter used --- Object Name of the object observed --- Patricia Bauer CDS 1998 Jun 25 Bifang LIU <bfliu@public.km.yn.cn> J_A+AS_132_83.xml On the Hipparcos photometry of Chemically Peculiar B, A, and F stars J/A+AS/132/93 J/A+AS/132/93 Hipparcos photometry of CP stars On the Hipparcos photometry of Chemically Peculiar B, A, and F stars S J Adelman Astron. Astrophys. Suppl. Ser. 132 93 1998 1998A&AS..132...93A I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Photometry Stars, early-type Stars, peculiar stars: chemically peculiar stars: early-type The Hipparcos photometry of the chemically peculiar main-sequence B, A and F stars are examined for variability. Some non-magnetic CP stars, Mercury-Manganese and metallic-line stars, which according to canonical wisdom should not be variable, may be variable and are identified for further study. Some potentially important magnetic CP stars are noted.
Hipparcos HgMn star photometry HR/HD HR (Cat. <V/50>) or HD (Cat. <III/135>) number --- HIP Hipparcos (Cat. <I/239>) number --- Hmag Average Hipparcos magnitude mag e_Hmag rms uncertainty on mag mag Amp Amplitude mag Comm Comments --- Hipparcos Am star photometry Hipparcos magnetic CP star photometry HD HD (Cat. <III/135>) number --- n_HD Note on the variability of the star number=1 *: known ellipsoidal variables and eclipsing binaries --- HIP Hipparcos (Cat. <I/239>) number --- Hmag Average Hipparcos magnitude mag e_Hmag rms uncertainty on mag mag Amp Amplitude mag Per Period d Patricia Bauer CDS 1998 Jun 29 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> J_A+AS_132_93.xml Stellar models for a wide range of initial chemical compositions until helium burning IV. From X=0.65 to X=0.80 for Z=0.004 J/A+AS/133/123 J/A+AS/133/123 Stellar models until He burning - IV. Stellar models for a wide range of initial chemical compositions until helium burning IV. From X=0.65 to X=0.80 for Z=0.004 A Claret A Gimenez Astron. Astrophys. Suppl. Ser. 133 123 1998 1998A&AS..133..123C J/A+AS/109/441 : Stellar models until He burning - I. (Claret, 1995) J/A+AS/114/549 : Stellar models until He burning - II. (Claret+, 1995) J/A+AS/125/439 : Stellar models until He burning - III. (Claret+, 1997) Models, evolutionary binaries: eclipsing Magellanic Clouds stars: evolution stars: interiors As a continuation of previous papers in a series devoted to the computation of stellar structure and evolution models we present a grid specifically obtained for detailed studies of the stellar content of the Small Magellanic Cloud. The initial metal content has thus been adopted to be Z=0.004 while the hydrogen content varies from 0.65 to 0.80 leaving as an intermediate value that given by standard laws of enrichment, X=0.744. Interpolation for different environment is therefore possible with these new models. Other input physics parameters, e.g. convective overshooting, mixing-length, opacities or nuclear reaction rates, have been adopted to be homogeneous with the previously published models in order to facilitate comparative studies.
All models with Z=0.04, X=0.65, 0.744 and 0.80 logM Initial mass of the model [solMass] X X initial composition (H) --- Z Z initial composition --- Overshoot without (0) or with (1) overshooting --- Age Age of models yr log(L) Total luminosity [solLum] log(g) Surface gravity [cm/s2] log(Teff) Effective temperature [K] log(k2) Apsidal motion constant (j=2) --- log(k3) Apsidal motion constant (j=3) --- log(k4) Apsidal motion constant (j=4) --- alpha alpha = -E_p_ x R/GM^2^ --- beta Fractional gyration radius ---- Patricia Bauer CDS 1998 Sep 07 Antonio Claret Dos Santos <claret@iaa.es> J_A+AS_133_123.xml Multi-Frequency Study of the B3-VLA Sample. I 10.6 GHz Data. J/A+AS/133/129 J/A+AS/133/129 B3-VLA sample 10.6 GHz data Multi-Frequency Study of the B3-VLA Sample. I 10.6 GHz Data. L Gregorini M Vigotti K -H Mack J Zonnchen U Klein Astron. Astrophys. Suppl. Ser. 133 129 1998 1998A&AS..133..129G VIII/37 : The Third Bologna Survey (B3) (Ficarra+ 1985) Radio sources Spectroscopy galaxies: general quasars: general radio continuum: general Table 1 presents the 10.6GHz fluxes of B3-VLA sample and an updated list of the Optical Identification of the sample.
B3-VLA sources at 10.6GHz B3 B3 name -- m_B3 Multiplicity index on B3 --- RAh Rigth ascension (B1950) h RAm Rigth ascension (B1950) min RAs Rigth ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec S10.6GHz Peak Flux at 10.6 GHz number=1 Peak flux is not given for the very complex sources that has been mapped and also for the upper limits. mJy I10.6GHz Integrated Flux at 10.6 GHz mJy l_I10.6GHz u means upper limit --- ID Optical Identification number=2 Q: quasar b: blue object F: featureless spectrum g: galaxy with redshift < 0.5 G: galaxy with redshift > 0.5 BL: BL Lac blank: Empty Fields --- Patricia Bauer CDS 1998 Aug 21 L. Gregorini <gregorini@astbo1.bo.cnr.it> J_A+AS_133_129.xml The Marseille Schmidt survey for active star-forming galaxies. I. Data on 92 emission line objects in two fields J/A+AS/133/171 J/A+AS/133/171 The Marseille Schmidt survey I. The Marseille Schmidt survey for active star-forming galaxies. I. Data on 92 emission line objects in two fields C Surace G Comte Astron. Astrophys. Suppl. Ser. 133 171 1998 1998A&AS..133..171S Active gal. nuclei Equivalent widths Galaxies, photometry galaxies: general galaxies: starburst methods: data analysis surveys We present data from a moderately deep spectroscopic Schmidt survey (B_lim_=17.5) of "active galaxies" selected by the presence of emission lines in their spectra and/or their UV excess. 92 emission line objects have been found in two adjacent fields (approximately 50deg^2^) in the direction of the southern extension of the Virgo cluster. We give a catalog containing positions, photographic R and B magnitudes, U-R colors, effective diameters, redshifts, equivalent widths and intensity ratios of the [OIII]{lambda}{lambda}4959,5007, H{beta} and [OII]{lambda}3727 emission lines. On these fields, we evaluate the completeness limit of the survey at a pseudo B magnitude values of 15.7. A more elaborate astrophysical analysis will appear in a forthcoming paper.
Catalog of the emission line objects Seq Sequential number in the catalog --- m_Seq Multiplicity index on Seq --- ID Identification in standard IAU notation --- m_ID Multiplicity index on ID --- Name Other name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Hvel Heliocentric velocity km/s e_Hvel Uncertainty on Hvel km/s Mclass Morphological classification number=1 Irr: Irregular galaxy cl: "clumpy" irregular HIIr: HII regions in an apparently normal spiral Sp: spirals (including galaxies with starburst nuclei) AGN: Active galactic nuclei SY1: Seyfert 1 SY2: Seyfert 2 LSB: Low surface brightness IP: interactive pair ?: unclassified B: barred object BC: blue compact --- Rmag R apparent magnitude mag RMAG R absolute magnitude mag U-R U-R (basel system) color mag Bmag B apparent magnitude mag EW[OIII] [OIII]5007+4959 Equivalent width 0.1nm EWHbeta Hbeta Equivalent width 0.1nm EW[OII] [OII]3727 Equivalent width 0.1nm [OIII]/Hb [OIII]/Hb line ratio --- [OII]/[OIII] [OII]/[OIII] line ratio --- Diameff R Effective diameter kpc charts.ps Finding charts table.ps PostScript version of the table table.tex LaTeX version of the table Patricia Bauer CDS 1998 Aug 21 Christian Surace <surace@mpia-hd.mpg.de> J_A+AS_133_171.xml CCD imaging of twenty nearby isolated irregular galaxies J/A+AS/133/181 J/A+AS/133/181 BVI imaging of 20 irregular galaxies CCD imaging of twenty nearby isolated irregular galaxies L Makarova I D Karachentsev Astron. Astrophys. Suppl. Ser. 133 181 1998 1998A&AS..133..181M J/A+AS/128/459 : BV photometry of irregular galaxies (Makarova+ 1998) J/A+AS/124/559 : VI photometry of dwarf galaxies (Karanchentsev+ 1997) Galaxies, photometry Photometry, CCD galaxies: distances and redshifts galaxies: dwarf galaxies: irregular galaxies: stellar content We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_<500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), >=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.
*List of galaxies RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin Gal Galaxy name --- VI photometry Gal Galaxy name --- Star Star number --- Xpos Rectangular coordinate of stars number=1 The upper right corner corresponds to X=0, Y=0 of the frame coordinates, i.e. X increases to East and Y to South. pix Ypos Rectangular coordinate of stars number=1 The upper right corner corresponds to X=0, Y=0 of the frame coordinates, i.e. X increases to East and Y to South. pix Vmag V magnitude mag V-I (V-I) colour index mag SHAR Sharpness parameter of stars number=2 SHAR is a measure of the difference between the observed width of the object and the width of the psf model. --- BV photometry Gal Galaxy name --- Star Star number --- Xpos Rectangular coordinate of stars number=1 The upper right corner corresponds to X=0, Y=0 of the frame coordinates, i.e. X increases to East and Y to South. pix Ypos Rectangular coordinate of stars number=1 The upper right corner corresponds to X=0, Y=0 of the frame coordinates, i.e. X increases to East and Y to South. pix Vmag V magnitude mag B-V (B-V) colour index mag SHAR Sharpness parameter of stars number=2 SHAR is a measure of the difference between the observed width of the object and the width of the psf model. --- Patricia Bauer CDS 1998 May 25 Sazonova Lida <lsaz@sao.ru> J_A+AS_133_181.xml uvby photometry of 33 Tauri, HD 50169, and HR 7786 and an assessment of FCAPT comparison stars J/A+AS/133/197 J/A+AS/133/197 uvby Photometry of 33 Tau, HD 50169 and HR 7786 uvby photometry of 33 Tauri, HD 50169, and HR 7786 and an assessment of FCAPT comparison stars S J Adelman C -L M Pi K Rayle Astron. Astrophys. Suppl. Ser. 133 197 1998 1998A&AS..133..197A J/A+AS/103/1 : ubvy photometry of magnetic CP stars (Adelman+ 1994) J/A+AS/106/333 : uvby photometry of four CP stars (Adelman+ 1994) J/A+AS/111/41 : Photometry of magnetic CP stars (North+, 1995) J/A+AS/114/253 : uvby Photometry of Magnetic CP Stars (Adelman+, 1995) J/A+AS/122/249 : uvby photometry of 4 CP stars (Adelman, 1997) J/A+AS/125/65 : uvby photometry of 4 CP stars (Adelman, 1997) J/A+AS/128/245 : Photometry of chemically peculiar stars (Adelman+ 1998) J/A+A/329/579 : uvby photometry of theta CrB (Fabregat+ 1998) Photometry, uvby Stars, peculiar stars: chemically peculiar stars: individual (33 Tau, HD 50169, HR 7786, HR 7721) Differential Stroemgren uvby photometric observations from the Four College Automated Photoelectric Telescope are presented for the ellipsoidal variable 33 Tauri, and the magnetic Chemically Peculiar stars HD 50169 and HR 7786. We confirm that Hube's period of 2.975272 days for 33 Tau is correct. HD 50169 is a constant MCP star. HR 7786 is a large amplitude class member confirming Winzer's discovery, but its period is 8.5297 days. Its comparison star, HR 7721, a spectroscopic binary B7 V star, is variable with an amplitude of order 0.1mag, but of indeterminant period. In addition Hipparcos photometry of the comparison and check stars for early type stars whose photometry is being obtained with the FCAPT is reviewed to ascertain the stability of these stars.
HD 24769 33 Tau 03 57 03.7 +23 10 32 HD 50169 06 51 59.2 -01 38 40 HR 7786 HD 193722 20 19 56.0 +46 50 14
Photometry of 33 Tau Photometry of HD 50169 Photometry of HR 7786 HJD Heliocentric Julian Date d u(v-c) variable-comparison (v-c) u magnitude mag u(ch-c) check-comparison (ch-c) u magnitude mag v(v-c) variable-comparison (v-c) v magnitude mag v(ch-c) check-comparison (ch-c) v magnitude mag b(v-c) variable-comparison (v-c) b magnitude mag b(ch-c) check-comparison (ch-c) b magnitude mag y(v-c) variable-comparison (v-c) y magnitude mag y(ch-c) check-comparison (ch-c) y magnitude mag Yearly means and standard deviations of tables 2, 3 & 4 Name Star name --- Per Period --- u(v-c) Variable-comparison (v-c) u magnitude mag e_u(v-c) rms uncertainty on u(v-c) mag u(ch-c) Check-comparison (ch-c) u magnitude mag e_u(ch-c) rms uncertainty on u(ch-c) mag v(v-c) Variable-comparison (v-c) v magnitude mag e_v(v-c) rms uncertainty on v(v-c) mag v(ch-c) Check-comparison (ch-c) v magnitude mag e_v(ch-c) rms uncertainty on v(ch-c) mag b(v-c) Variable-comparison (v-c) b magnitude mag e_b(v-c) rms uncertainty on b(v-c) mag b(ch-c) Check-comparison (ch-c) b magnitude mag e_b(ch-c) rms uncertainty on b(ch-c) mag y(v-c) Variable-comparison (v-c) y magnitude mag e_y(v-c) rms uncertainty on y(v-c) mag y(ch-c) Check-comparison (ch-c) y magnitude mag e_y(ch-c) rms uncertainty on y(ch-c) mag Hipparcos Photometry for Groups of B, A, and F stars. Var Variable star name(s) --- Varmag Mean magnitude of star Var mag e_Varmag rms uncertainty on Varmag mag VarAmp Amplitude of star Var mag VarComm Comments for star Var --- Comp Comparison star name(s) --- Compmag Mean magnitude of star Comp mag e_Compmag rms uncertainty on Compmag mag CompAmp Amplitude of star Comp mag CompComm Comments for star Comp --- ch Check star name(s) --- chmag Mean magnitude of ch star mag e_chmag rms uncertainty on chmag mag chAmp Amplitude of ch star mag chCom Comments for ch star --- oc Old comparison star name (s) --- ocmag Mean magnitude of oc star mag e_ocmag rms uncertainty on ocmag mag ocAmp Amplitude of oc star mag oh Old check star name(s) --- ohmag Mean magnitude of oh star mag e_ohmag rms uncertainty on ohmag mag ohamp Amplitude of oh star mag ocComm Comments for oh star --- Patricia Bauer CDS 1998 Jun 02 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> J_A+AS_133_197.xml New variable chemically peculiar stars identified in the Hipparcos archive J/A+AS/133/1 J/A+AS/133/1 New variable chemically peculiar stars New variable chemically peculiar stars identified in the Hipparcos archive E Paunzen H M Maitzen Astron. Astrophys. Suppl. Ser. 133 1 1998 1998A&AS..133....1P III/162 : General Catalogue of Ap and Am stars (Renson+ 1991) III/199 : Observed Periods of Ap and Bp stars (Catalano+ 1998) I/196 : Hipparcos Input Catalogue, Version 2 (Turon+ 1993) J/A+AS/121/57 : Ap stars periodicity (Catalano+ 1997) J/A+AS/128/573 : ubvy{Delta}a photometry of Renson stars (Maitzen+ 1998) Rotational velocities Stars, peculiar Stars, variable stars: chemically peculiar stars: early-type stars: variables: general Since variability of chemically peculiar (CP) stars plays an important role for the astrophysical explanation of their outstanding behaviour, we have identified new variable CP stars listed in Renson's catalogue using the extensive Hipparcos Variability Annex. From the 293 objects found, 33 were excluded because they are not CP stars and/or have no period listed, half of the remaining stars are newly identified and half had been already included in the catalogue of variable CP stars by Catalano & Renson (1997, Cat. <J/A+AS/121/57>). Most of the newly identified variability is due to an apparent magnetic field coupled with stellar rotation (oblique rotator model). The constraints of this model are fulfilled for all but three CP2 stars. Variations of bona fide Am-Fm stars are exclusively explained by eclipses of binary systems. Furthermore eight candidates of the gamma Doradus group (pulsating Am-Fm stars) were detected. Table 1 (table1.dat) presents the newly identified chemically peculiar stars.
New variable chemically peculiar stars identified in the Hipparcos archive HD HD number with probability mark according to Renson (1991) --- n_HD Probability mark according to Renson (1991, Cat. <III/162>) number=1 Indication of the probability that the star belongs to the considered category: '/' denotes a star improperly considered Ap or Am '?' doubtful nature '*' well-known Ap or Am star ' ' other cases --- HIC HIC (Cat. <I/196>) number --- RNS Number from Renson (1991, Cat. <III/162>) --- Type Type of variations --- Min Minimum of the variations mag l_Max Limit flag on Max --- Max Maximum of the variations mag Period Period of the variations d Epoch Epoch as in the HVA (Hipparcos Variability Annex) d Deltaa {Delta}a index number=2 {Delta}a is a photometric index that measure the intensity of the depression at {lambda}5200{AA}. All stars with {Delta}a>=0.010mag are considered as peculiar stars. See Maitzen et al., 1976A&A....51..223M, for more details. mmag Deltap {Delta}p index number=3 {Delta}p is a photometric index, depending of (b-y), m_1_, c_1_ and {beta} photometry, able to detect CP2 stars. See Masana et al., Cat. <J/A+AS/128/265>, for more details. --- l_vsini Limit flag on vsini --- vsini vsini value km/s Spec Spectral type according to Renson (1991, Cat. <III/162>)) --- Patricia Bauer CDS 1998 Oct 01 E. Paunzen <PAUNZEN@astro.ast.univie.ac.at> J_A+AS_133_1.xml Spectral classification of unidentified IRAS point sources with F_{nu}_(12{mu}m) >= F_{nu}_(25{mu}m). J/A+AS/133/201 J/A+AS/133/201 Spectral class. of unidentified IRAS sources Spectral classification of unidentified IRAS point sources with F_{nu}_(12{mu}m) >= F_{nu}_(25{mu}m). K V K Iyengar D J MacConnell Astron. Astrophys. Suppl. Ser. 133 201 1998 1998A&AS..133..201I II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) II/177 : Near IR Photometry of a Sample of IRAS Point Sources (Fouque+ 1992) III/197 : IRAS Low Resolution Spectra (IRAS team, 1987) J/A+AS/90/327 : 1612MHz OH survey of IRAS point sources (te Lintel Hekkert+ 1991) J/A+A/299/453 : OH/IR stars photometry (Lepine+, 1995) J/A+AS/99/31 : Identification of C stars in IRAS (Guglielmo+ 1993) J/ApJ/411/188 : Classification of bright IRAS variables (Allen+ 1993) Infrared sources Spectral types infrared: stars stars: AGB and post-AGB stars: carbon stars: late-type stars: mass-loss M spectral types and IRAS infrared magnitudes, colors, and variability parameters are given for 155 largely unidentified IRAS point sources having quality-3 flux densities at 12, 25, and 60 mum.
IRAS
Spectral type of IRAS unidentified sources which have quality-3 flux density data at 12, 25, and 60 {mu}m IRAS IRAS Point Source (Cat. <II/125>) name --- Footnote Optional footnote to entry number=1 References: a: Allen et al., 1993, Cat. <J/ApJ/411/188> b: Fouque et al., 1992, Cat. <II/177> c: Guglielmo et al., 1993, Cat. <J/A+AS/99/31> d: Haikala et al., 1994A&AS..103..107H e: Hashimoto, 1994, Cat. <J/A+AS/107/445> f: Jiang et al., 1996, Cat. <J/ApJS/106/463> g: Lepine et al., 1995, Cat. <J/A+A/299/453> h: Lewis et al., 1990ApJ...362..634L i: Olnon et al., 1986A&AS...65..607O j: Sivagnanam et al., 1990A&A...233..112S k: te Lintel Hekkert et al., 1991, Cat. <J/A+AS/90/327> l: Volk et al., 1991ApJS...77..607V m: Kwok et al., 1997ApJS..112..557K --- GLON Galactic longitude deg GLAT Galactic latitude deg SpType Spectral type by DJM number=2 Classification of MacConnell, 1992AJ....104..821M --- [12] IRAS magnitude at 12 mum mag [25] IRAS magnitude at 25 mum mag [60] IRAS magnitude at 60 mum mag ([12]-[25])VH IRAS color number=3 Colours as defined by van der Veen and Habing (1988A&A...194..125V): [12]-[25]=2.5[log(F_nu_(25)/F_nu_(12))] [25]-[60]=2.5[log(F_nu_(60)/F_nu_(25))] mag ([25]-[60])VH IRAS color number=3 Colours as defined by van der Veen and Habing (1988A&A...194..125V): [12]-[25]=2.5[log(F_nu_(25)/F_nu_(12))] [25]-[60]=2.5[log(F_nu_(60)/F_nu_(25))] mag Var IRAS variability flag --- LRS IRAS Low-Resol. Spectrometer flag --- table6.tex LaTeX version of table6 table6.ps PostScript version of table6 Patricia Bauer CDS 1998 Oct 28 Jack MacConnell <MACCONNELL@stsci.edu> J_A+AS_133_201.xml Stark broadening of spectral lines of multicharged ions of astrophysical interest. XXII: K VIII and K IX spectral lines J/A+AS/133/227 J/A+AS/133/227 Stark broadening of K VIII and K IX Stark broadening of spectral lines of multicharged ions of astrophysical interest. XXII: K VIII and K IX spectral lines M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 133 227 1998 1998A&AS..133..227D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines J/A+AS/127/295 : Stark broadening of Kr II lines J/A+AS/127/543 : Stark broadening of S V lines J/A+AS/128/203 : Stark broadening of Mn, Ga & Ge multiplets J/A+AS/128/359 : Stark broadening of Ca IX and Ca X lines J/A+AS/129/155 : Stark broadening of Si XI and Si XIII lines J/A+AS/130/539 : Stark broadening of Na X Atomic physics atomic data line: profiles By using the semiclassical-perturbation formalism, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 K VIII and 30 K IX multiplets, of interest for analysis, investigation and modeling of different plasmas in solar and stellar subphotospheric layers research and plasma physics. The obtained results are presented as a function of temperature and perturber density. Results are compared with other theoretical estimates, based on regularities and systematic trends.
Stark broadening parameters due to e-, p- and He III-impacts for K VIII Stark broadening parameters due to e-, p- and He III-impacts for K IX N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dp shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dHe++ shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1998 Jun 08 Dr Milan Dimitrijevic <mdimitrijevic@aob.bg.ac.yu> J_A+AS_133_227.xml Recombination coefficients for Ne II lines at nebular temperatures and densities J/A+AS/133/257 J/A+AS/133/257 Recombination coefficients for NeII lines Recombination coefficients for Ne II lines at nebular temperatures and densities R Kisielius P J Storey A R Davey L T Neale Astron. Astrophys. Suppl. Ser. 133 257 1998 1998A&AS..133..257K VI/64 : Recombination line intensities for hydrogenic ions (Storey+ 1995) Atomic physics atomic data HII regions planetary nebulae: general We calculate total recombination coefficients for Ne^2+^ + e^-^ and effective recombination coefficients for the formation of selected lines of Ne II. New photoionization data are calculated which accurately map the near threshold resonances and are used to derive recombination coefficients for principal quantum numbers, n<=15, including radiative and dielectronic recombination. Cascading from higher states is included, allowing for the effects of finite electron density in a hydrogenic approximation. The effects of population in the excited states of the recombining ion are investigated.
Comparison of calculated and experimental energies for the Ne^2+^ target states. Config Electronic configuration --- Term State term --- Epresent Present calculation energy of term Ry Eexperimental Experimental energy of term Ry Total recombination coefficients T Electron temperature K Case Plasma state case number=1 In Case A, all emission lines are assumed to be optically thin. In Case B, lines terminating on the ^2^P^o^ term are assumed to be thick and no radiative decays to this state arte permitted when calculating the population structure. See Baker & Menzel, (1938ApJ....88...52B) for more details. --- RC2 Recombination coefficients at N_e_=10^2^cm^-3^ 10-12cm3/s RC4 Recombination coefficients at N_e_=10^4^cm^-3^ 10-12cm3/s RC5 Recombination coefficients at N_e_=10^5^cm^-3^ 10-12cm3/s RC6 Recombination coefficients at N_e_=10^6^cm^-3^ 10-12cm3/s Effective recombination coefficients at electron density N_e_=10^4^cm^-3^. Effective recombination coefficients at electron density N_e_=10^6^cm^-3^. SP1 2S+1 of upper state parent term --- LP1 L of upper state parent term --- PP1 Parity of upper state parent term number=1 0 for even, 1 for odd --- n1 Principal quantum number of outer electron --- l1 Orbital quantum number of outer electron --- S1 2S+1 of upper state term --- L1 L of upper state term --- P1 Parity of upper state term number=1 0 for even, 1 for odd --- SP2 2S+1 of lower state parent term --- LP2 L of lower state parent term --- PP2 Parity of lower state parent term number=1 0 for even, 1 for odd --- n2 Principal quantum number of outer electron --- l2 Orbital quantum number of outer electron --- S2 2S+1 of lower state term --- L2 L of lower state term --- P2 Parity of lower state term number=1 0 for even, 1 for odd --- Case Plasma state case number=2 In Case A, all emission lines are assumed to be optically thin. In Case B, lines terminating on the ^2^P^o^ term are assumed to be thick and no radiative decays to this state arte permitted when calculating the population structure. See Baker & Menzel, (1938ApJ....88...52B) for more details. --- lambda Transition wavelength in nm nm ECR1 Te= 1000K effective recombination coefficient 10-14cm3/s ECR2 Te= 2000K effective recombination coefficient 10-14cm3/s ECR3 Te= 3000K effective recombination coefficient 10-14cm3/s ECR5 Te= 5000K effective recombination coefficient 10-14cm3/s ECR75 Te=75000K effective recombination coefficient 10-14cm3/s ECR100 Te=10000K effective recombination coefficient 10-14cm3/s ECR125 Te=12500K effective recombination coefficient 10-14cm3/s ECR150 Te=15000K effective recombination coefficient 10-14cm3/s ECR200 Te=20000K effective recombination coefficient 10-14cm3/s Fitting coefficients and maximum fitting errors(%) for effective recombination coefficients. Electron density N_e_=10^4^cm^-3^. SP1 2S+1 of upper state parent term --- LP1 L of upper state parent term --- PP1 Parity of upper state parent term number=1 0 for even, 1 for odd --- n1 Principal quantum number of outer electron --- l1 Orbital quantum number of outer electron --- S1 2S+1 of upper state term --- L1 L of upper state term --- P1 Parity of upper state term number=1 0 for even, 1 for odd --- SP2 2S+1 of lower state parent term --- LP2 L of lower state parent term --- PP2 Parity of lower state parent term number=1 0 for even, 1 for odd --- n2 Principal quantum number of outer electron --- l2 Orbital quantum number of outer electron --- S2 2S+1 of lower state term --- L2 L of lower state term --- P2 Parity of lower state term number=1 0 for even, 1 for odd --- Case Plasma state case number=2 In Case A, all emission lines are assumed to be optically thin. In Case B, lines terminating on the ^2^P^o^ term are assumed to be thick and no radiative decays to this state arte permitted when calculating the population structure. See Baker & Menzel, (1938ApJ....88...52B) for more details. --- Lambda Transition wavelength in nm nm a Fitting coefficient a number=3 Fit parameters and maximum deviations from the calculated data are given for the effective recombination coefficients at N_e_=10^4^cm^-3^. The coefficients are fitted by a least-squares algorithm to the functional form: {alpha}_eff_=10^-14^*at^f^(1+b(1-t)+c(1-t)^2^+d(1-t)^3^), where t=T_e_[K]/10^4^, and a, b, c, d and f are constants. Fitting is valid for the whole temperature range studied for all lines except those denoted by asterisk in the last column. 10-14cm3/s b Fitting coefficient b number=3 Fit parameters and maximum deviations from the calculated data are given for the effective recombination coefficients at N_e_=10^4^cm^-3^. The coefficients are fitted by a least-squares algorithm to the functional form: {alpha}_eff_=10^-14^*at^f^(1+b(1-t)+c(1-t)^2^+d(1-t)^3^), where t=T_e_[K]/10^4^, and a, b, c, d and f are constants. Fitting is valid for the whole temperature range studied for all lines except those denoted by asterisk in the last column. 10-14cm3/s c Fitting coefficient c number=3 Fit parameters and maximum deviations from the calculated data are given for the effective recombination coefficients at N_e_=10^4^cm^-3^. The coefficients are fitted by a least-squares algorithm to the functional form: {alpha}_eff_=10^-14^*at^f^(1+b(1-t)+c(1-t)^2^+d(1-t)^3^), where t=T_e_[K]/10^4^, and a, b, c, d and f are constants. Fitting is valid for the whole temperature range studied for all lines except those denoted by asterisk in the last column. 10-14cm3/s d Fitting coefficient d number=3 Fit parameters and maximum deviations from the calculated data are given for the effective recombination coefficients at N_e_=10^4^cm^-3^. The coefficients are fitted by a least-squares algorithm to the functional form: {alpha}_eff_=10^-14^*at^f^(1+b(1-t)+c(1-t)^2^+d(1-t)^3^), where t=T_e_[K]/10^4^, and a, b, c, d and f are constants. Fitting is valid for the whole temperature range studied for all lines except those denoted by asterisk in the last column. 10-14cm3/s f Fitting coefficient f number=3 Fit parameters and maximum deviations from the calculated data are given for the effective recombination coefficients at N_e_=10^4^cm^-3^. The coefficients are fitted by a least-squares algorithm to the functional form: {alpha}_eff_=10^-14^*at^f^(1+b(1-t)+c(1-t)^2^+d(1-t)^3^), where t=T_e_[K]/10^4^, and a, b, c, d and f are constants. Fitting is valid for the whole temperature range studied for all lines except those denoted by asterisk in the last column. 10-14cm3/s FitErr Maximum fitting error (in percent) % Note Asterisks denote line for which fitting is valid from T_e_=2000K. --- The factors b(J_i_,J_f_) and wavelengths(in air) for the strongest multiplets of Ne II. Trans Transition multiplet --- Si 2S+1 of upper term --- Li L of upper term --- --- --- Ji J of upper term --- Sf 2S+1 of lower term --- Lf L of lower term --- --- --- Jf J of lower term --- Lambda Wavelength of transition line nm b(Ji,Jf) Splitting factor b(Ji,Jf) defined by Eq.(10). --- Patricia Bauer CDS 1998 Jul 02 Dr. Romas Kisielius <rk@aura.phys.ucl.ac.uk> J_A+AS_133_257.xml CCD photometry of distant open clusters. IV. Trumpler 5. J/A+AS/133/25 J/A+AS/133/25 CCD BVI photometry of Trumpler 5 CCD photometry of distant open clusters. IV. Trumpler 5. J Kaluzny Astron. Astrophys. Suppl. Ser. 133 25 1998 1998A&AS..133...25K J/A+AS/108/151 : Berkeley 22 & Berkeley 29 CCD photometry (Kaluzny, 1994) J/A+AS/114/1 : CCD UBVI photometry of NGC 6791 (Kaluzny+, 1995) J/A+AS/121/455 : BVI photometry of stars in Berkeley 18 (Kaluzny 1997) Clusters, open Photometry, CCD Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Trumpler 5) BVI data for stars from the field of the old open cluster Tr 5 are given
Cl Trumpler 15 10 44.8 -59 22
VI data obtained with the 2.1m KPNO telescope on November 11, 1990 Seq Sequential number --- Xpos X coordinate number=1 1 pixel=0.30 arcsec. X axis points toward South, Y axis points toward East. pix Ypos Y coordinate number=1 1 pixel=0.30 arcsec. X axis points toward South, Y axis points toward East. pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag o_Vmag Number of averaged V measurements --- q_Vmag Quality flag for V number=2 q=1 means relatively poor quality --- V-I V-I colour index mag e_V-I rms uncertainty on V-I mag o_V-I Number of averaged I measurements --- q_V-I Quality flag for V-I number=2 q=1 means relatively poor quality --- BV data obtained with the 2.1m KPNO telescope on October 06, 1991 BV data obtained with the 0.9mm KPNO telescope on October 11 & 12, 1991 Seq Sequential number --- Xpos X coordinate number=1 1 pixel=0.68 arcsec, X axis points toward North, Y axis points toward East pix Ypos Y coordinate number=1 1 pixel=0.68 arcsec, X axis points toward North, Y axis points toward East pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag o_Vmag Number of averaged V measurements --- q_Vmag Quality flag for V number=2 q=1 means relatively poor quality --- B-V B-V colour index mag e_B-V rms uncertainty on B-V mag o_Bmag Number of averaged B measurements --- q_B-V Quality flag for B-V number=2 q=1 means relatively poor quality --- Patricia Bauer CDS 1998 Aug 28 Janusz Kaluzny <jka@vela.astrouw.edu.pl> J_A+AS_133_25.xml Long-term spectroscopy of eta Carinae. I. The high and low excitation phases J/A+AS/133/299 J/A+AS/133/299 Long-term spectroscopy of eta Carinae Long-term spectroscopy of eta Carinae. I. The high and low excitation phases A Damineli O Stahl A Kaufer B Wolf G Quast D F Lopes Astron. Astrophys. Suppl. Ser. 133 299 1998 1998A&AS..133..299D Radial velocities Spectroscopy Stars, Be binaries: general Hertzsprung-Russell (HR diagram) stars: emission-line, Be stars: individual (eta Car) This Table contains parameters of 655 spectral features in the spectrum of eta Carinae, in the wavelength region 3850-11000 Angstrom. The narrow and broad line components were measured separately, for the spectrum in high excitation state (year 1995) and during the "spectroscopic event" of June/1992. The spectra were collected at ESO (Chile) and LNA (Brazil) at high resolution. Several spectral lines of Fe II, [Fe II], [Fe III], [N II] ands Ca II are identifyed for the first time in the spectrum of this star. Line variability between high and low excitation states is characterized in an objective way (parameter var in the last column).
eta Car HD 93308 10 45 03.6 -59 41 03
List of measurements Name Reference name for the feature --- Ident Identification of the atomic transition --- Com Commentary on the appearance of the feature --- LambdaLab Laboratory wavelength of the atomic transition 0.1nm n_LambdaLab Note on LambdaLab number=1 ]: For lines that have no identification, the observed wavelength was corrected by the radial velocity of the object (-40 km/s) in order to indicate the expected laboratory wavelength. --- LamObs1 Observed wavelength of the feature (1995) 0.1nm n_LamObs1 ND when not detected --- HRV1 Heliocentric radial velocity (1995) km/s u_HRV1 Uncertainty flag on HRV1 --- I/Ic1 Relative intensity of line peak to the continuum (1995) --- n_I/Ic1 ND when not detected --- Flux1 Line flux relative to the local continuum (1995) - number=2 This is equal to the equivalent width in Angstrom for lines seated on the stellar continuum. --- fwhm1 Full width at half maximum (1995) km/s LamObs2 Observed wavelength of the feature (June/1992) 0.1nm n_LamObs2 ND when not detected --- HRV2 Heliocentric radial velocity (June/1992) km/s I/Ic2 Relative intensity of line peak to continuum (June/1992) --- Flux2 Line flux relative to the local continuum (June/1992) - number=2 This is equal to the equivalent width in Angstrom for lines seated on the stellar continuum. --- fwhm2 Full width at half maximum (June/1992) km/s var Line variability from high to low states number=3 Defined in equation (1) - see text --- table1.ps PostScript version of table1 table1.tex LaTeX version of table1 A. Damineli IAG-USP A. Kaufer Landessternwarte 1998 Jun 22 Andreas Kaufer <A.Kaufer@lsw.uni-heidelberg.de> J_A+AS_133_299.xml A survey of molecular line emission towards ultracompact HII regions J/A+AS/133/29 J/A+AS/133/29 Molecular line survey towards UC HII A survey of molecular line emission towards ultracompact HII regions J Hatchell M A Thompson T J Millar G H Macdonald Astron. Astrophys. Suppl. Ser. 133 29 1998 1998A&AS..133...29H J/A+AS/120/283 : Water maser features in UC HII regions (Hofner+ 1996) H II regions Radio lines HII regions ISM: clouds ISM: molecules molecular processes radio lines: ISM stars: formation The tables give identifications for molecular lines detected in the survey of ultracompact HII regions. The survey covers 14 sources: G5.89, G9.62, G10.30, G10.47, G12.21, G13.87, G29.96, G31.41, G34.26, G43.89, G45.12, G45.45, G45.47, and G75.78. For each source, we observed up to ten 1~GHz bands between 200 and 350~GHz, covering lines of more than 30 species including multiple transitions of CO isotopes, CH_3_OH, CH_3_CCH, CH_3_CN and HCOOCH_3, and sulphuretted molecules. The tables give the measured line parameters of observed frequency {nu}(obs), peak temperature T_R_^*^ and linewidth {Delta}{nu}_1/2_ for each line. Each independent detection of a particular line is given. The species, transition, rest frequency and upper level energy (E_u_/k) are given for identified lines.
G9.62 [WC89] 009.62+0.19 18 06 14.9 -20 31 40 G10.30 [WC89] 010.30-0.15 18 08 56.0 -20 05 54 G10.47 [WC89] 010.47+0.03 18 08 38.3 -19 51 50 G12.21 [WC89] 012.21-0.10 18 12 39.6 -18 24 21 G13.87 [HC96] G13.87+0.28 18 14 35.5 -16 45 38 G29.96 [WC89] 029.96-0.02 18 46 03.8 -02 39 22 G31.41 [WC89] 031.41+0.31 18 47 34.5 -01 12 43 G34.26 [HC96] G34.26+0.15 18 53 18.4 +01 14 58 G43.89 [WC89] 043.89-0.78 19 14 26.1 +09 22 34 G45.12 [WC89] 045.12+0.13 19 13 27.8 +10 53 37 G45.45 [WC89] 045.45+0.06 19 12 00.1 +11 04 00 G45.47 [WC89] 045.47+0.05 19 14 25.5 +11 09 26 G75.78 [WC89] 075.78+0.34 20 21 44.0 +37 26 40
Molecular lines observed toward 8 UC HII Molecular lines observed towards the line poor sources Name HII region name --- n_Name Note for G34.26 observations number=1 *: Molecular lines observed towards G34.26 at offset positions. The lines before the break were observed at (0,20) offset from the centre position and the lines after the break were observed at (20,0) offset from the centre position. --- nuObs Observed centre frequency of line GHz TR* Peak brightness temperature of line K Dnu1/2 FWHM of line MHz Species Species identified for transition --- Trans Quantum numbers of transition --- nuRest Rest frequency of transition GHz Eu/k Upper state energy of transition divided by Boltzmann constant K Notes Notes number=2 This column gives further information about the line in the form of one or more codes. blend: blended line self-abs: self-absorbed line sba: line which has a sideband ambiguity sl-blend: when it has been possible to extract lines from blends Some HCOOCH_3_, C_2_H_5_OH and H_2_CCHCN lines are blends of two or transitions of the same frequency and are indicated as such by blend. *: All possibilities for uncertain detections are given, with the most likely indicated by an asterisk. --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Aug 10 Jennifer Hatchell <j.hatchell@umist.ac.uk> J_A+AS_133_29.xml Stellar kinematical data for the central region of spiral galaxies J/A+AS/133/317 J/A+AS/133/317 Stellar kinematical data in spiral galaxies Stellar kinematical data for the central region of spiral galaxies P Heraudeau F Simien Astron. Astrophys. Suppl. Ser. 133 317 1998 1998A&AS..133..317H Galaxies, rotation Radial velocities Rotational velocities Velocity dispersion galaxies: general galaxies: kinematics and dynamics galaxies: spiral We present the results of absorption spectroscopy on the inner region of 34 Sa-Sc galaxies. We have determined the central velocity dispersion and, for 32 of these objects, stellar rotation curves and velocity-dispersion profiles. Some of these profiles are limited to the bulge, some others do reach a region dominated by the luminosity of the disk. These data are intended to provide basic material for the study of the mass distribution and dynamical status in the central regions of spiral galaxies. Although no elaborate bulge-and-disk photometric decomposition is performed, we estimate the effects of limited resolution and contamination by disk light on the central velocity dispersion of the bulge.
Catalog elements and kinematical results Name Object identification --- Mtype Morphological type Parameters Mtype through Mb are catalog elements from the LEDA database (status: LEDA1998). Parameters HRV through fbulge are determinations of the present work --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Btc Corrected integrated blue magnitude mag D25 Diameter at 25 B mag/arcsec**2 arcmin Eps Ellipticity --- PA Position angle of major axis PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1996). deg Mb Absolute blue magnitude Mb calculated from Btc and kinematical distance modulus, with H=75km/s/Mpc mag HRV Heliocentric radial velocity km/s u_HRV Uncertainty flag on HRV --- e_HRV Mean error on HRV km/s sig0 Central velocity dispersion km/s u_sig0 Uncertainty flag on sig0 --- e_sig0 Mean error on sig0 km/s fbulge Resolution effect on bulge kinematics Factor indicating the degree to which resolution effects and contamination by disk light have influenced the observed central bulge kinematics; {sigma}_0_/fbulge is then a closer approximation to the averaged, luminosity weighted bulge velocity dispersion within 0.1r_e_ (see Sect. 5 and the Appendix). --- Log of the observations Name Object identification --- Date Date of observation (dd/mm/yy) "DD/MM/YY" Setup Spectrograph setup Setup=1 corresponds to a dispersion of 66 Angtroems per mm Setup=2 corresponds to a dispersion of 33 Angtroems per mm --- PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with the following convention on the subsequent radius r in the profiles (Table 3): - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg Nexp Number of exposures --- Texp Exposure time min Seeing Seeing FWHM arcsec u_Seeing Uncertainty flag on Seeing --- Profiles of velocity dispersion and rotation Name Object identification --- PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg r Radius (<0 and >0 on opposite semi-axes) arcsec Vrot Proj. mean stellar rotation velocity Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. km/s e_Vrot Mean error on Vrot km/s sigma Projected velocity dispersion km/s e_sigma Mean error on sigma km/s Patricia Bauer CDS 1998 Oct 08 Francois Simien <fs@cumulus.univ-lyon1.fr> J_A+AS_133_317.xml Extended stellar kinematics of elliptical galaxies in the Fornax cluster J/A+AS/133/325 J/A+AS/133/325 Velocities of 12 Fornax elliptical galaxies Extended stellar kinematics of elliptical galaxies in the Fornax cluster A W Graham M M Colless G Busarello S Zaggia G Longo Astron. Astrophys. Suppl. Ser. 133 325 1998 1998A&AS..133..325G II/180 : Galaxies in 3.5degs of Fornax cluster, and in 5 nearby groups J/A+AS/106/199 : B-band photometry in Fornax and Virgo (Caon+ 1994) J/A+A/296/319 : Fornax cluster early-type galaxies (D'Onofrio+, 1995) Clusters, galaxy Rotational velocities Velocity dispersion galaxies: clusters: individual (Fornax cluster) galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: kinematics and dynamics galaxies: structure We present extended stellar kinematics for a sample of elliptical galaxies in the Fornax cluster. Out of the 13 galaxies presented here, five (FCC 119, FCC 136, NGC 1373, NGC 1428, FCC 335) have no previously published kinematical data. Major-axis velocity dispersion profiles (VDPs) and rotation curves (RCs) are given for 12 of the galaxies. A major feature of this data is the spatial extension: for 8 galaxies the data extends beyond 1R_e_, and for 5 it extends beyond 2R_e_. Compared to the previously available data, this corresponds to an increase in spatial coverage by a factor from 1 to 5. The present sample represents 86% of the ellipticals in Fornax brighter than B_T_=15mag.
List of galaxies (file added at CDS) RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Name Galaxy Name --- Major axis kinematics Name Galaxy name --- m_Name Multiplicity index on name --- r Distance from the center (r>0 means Eastwards) arcsec V(r) Rotation velocity along the major axis km/s e_V(r) rms uncertainty on V(r) km/s DV(r) Velocity dispersion along the major axis km/s e_DV(r) rms uncertainty on DV(r) km/s Patricia Bauer CDS 1998 Sep 07 Gianni Busarello <gianni@na.astro.it> Alister Graham <ali@mso.anu.edu.au> J_A+AS_133_325.xml Studies of dense molecular cores in regions of massive star formation. VII. Core properties on the galactic scale J/A+AS/133/337 J/A+AS/133/337 Dense molecular cores. VII. Studies of dense molecular cores in regions of massive star formation. VII. Core properties on the galactic scale I Zinchenko L Pirogov M Toriseva Astron. Astrophys. Suppl. Ser. 133 337 1998 1998A&AS..133..337Z J/A+A/288/601 : Dense molecular cores. I. (Zinchenko+ 1994) J/A+AS/111/95 : Dense molecular cores. II. (Zinchenko+, 1995) J/A+AS/118/191 : Dense molecular cores. IV. (Juvela 1996) J/A+AS/124/385 : Dense molecular cores. V. (Zinchenko+ 1997) Zinchenko, Paper III 1995A&A...303..554Z Lapinov et al., Paper VI 1998A&A...336.1007L Masers Radio lines ISM: clouds ISM: molecules radio lines: ISM stars: formation We searched the IRAS point source catalogue (Cat. <II/125>) for possible associations with our targets. In table 2, we list the sources from this catalogue located within 5' from the maser positions. They are present in all cases except G 145.39+4.00.
Source list Name Maser source name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Names Other names --- IRAS point sources within 5' from the maser positions GLON Galactic longitude of maser deg GLAT Galactic latitude of maser deg opos Angular offset from the maser position arcsec IRAS IRAS point source name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign (B1950) --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec F(12) Flux at 12 microns Jy F(25) Flux at 25 microns Jy F(60) Flux at 60 microns Jy F(100) Flux at 100 microns Jy Q(12) Quality flag at 12 microns --- Q(25) Quality flag at 25 microns --- Q(60) Quality flag at 60 microns --- Q(100) Quality flag at 100 microns --- Patricia Bauer CDS 1998 Jun 25 Igor Zinchenko <igor@zin.appl.sci-nnov.ru> J_A+AS_133_337.xml Determination of proper motions and membership of the open clusters NGC 1817 and NGC 1807 J/A+AS/133/387 J/A+AS/133/387 NGC 1817 and NGC 1807 proper motions Determination of proper motions and membership of the open clusters NGC 1817 and NGC 1807 L Balaguer-Nunnez K P Tian J L Zhao Astron. Astrophys. Suppl. Ser. 133 387 1998 1998A&AS..133..387B I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) I/146 : Positions and Proper Motions - North (Roeser+, 1988) Clusters, open Proper motions astrometry open clusters and associations: individual (NGC 1817, NGC 1807) Relative proper motions, their corresponding errors and membership probabilities of 722 stars in the open cluster NGC 1817 region are given. Equatorial coordinates were computed using Tycho Catalog (Cat. <I/239>) as reference stars. Forty stars from this catalog are in the region under study. The cross-identification of this 40 stars are given as notes. Only 15 stars were found in this region from the PPM Catalog (Cat. <I/146>), and their respective identification is also included in the note5.dat file.
Relative proper motions and membership probabilities of 722 stars of NGC 1817 and NGC 1807 Seq Sequential identification number --- xpos x-plate coordinate (towards East) cm ypos y-plate coordinate (towards North) cm RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec pmx Proper motion in x mas/yr pmy Proper motion in y mas/yr e_pmx error in PMx mas/yr e_pmy error in PMy mas/yr Pngc1817 Probability NGC 1817 cluster star --- Pngc1807 Probability NGC 1807 cluster star --- Pfield Probability Field star --- W Number of plate pairs used --- TYC Tycho (Cat. <I/239>) number --- PPM PPM (Cat. <I/146>) number --- Patricia Bauer CDS 1998 Jul 02 Lola Balaguer-Nunnez <lbalague@pchpc3.am.ub.es> J_A+AS_133_387.xml Ionization balance for optically thin plasmas: rate coefficients for all atoms and ions of the elements H to Ni. J/A+AS/133/403 J/A+AS/133/403 Ionization balance for optically thin plasmas Ionization balance for optically thin plasmas: rate coefficients for all atoms and ions of the elements H to Ni. P Mazzotta G Mazzitelli S Colafrancesco N Vittorio Astron. Astrophys. Suppl. Ser. 133 403 1998 1998A&AS..133..403M Atomic physics atomic data plasmas radiation mechanisms: thermal X-rays: general Fitting coefficients for dielectronic recombination rates of formula (7) of the paper are detailed in two tables.
Fitting coefficients for dielectronic recombination rates Ion Ion's label --- c1 c1 coefficient cm3/s c2 c2 coefficient cm3/s c3 c3 coefficient cm3/s c4 c4 coefficient cm3/s E1 E1 coefficient cm3/s E2 E2 coefficient cm3/s E3 E3 coefficient cm3/s E4 E4 coefficient cm3/s Ionization equilibrium El Element symbol --- logT Temperature (log_10_(T)) [K] LogX1 Ionic fraction for Element I (neutral) --- LogX2 Ionic fraction for Element II --- LogX3 Ionic fraction for Element III --- LogX4 Ionic fraction for Element IV --- LogX5 Ionic fraction for Element V --- LogX6 Ionic fraction for Element VI --- LogX7 Ionic fraction for Element VII --- LogX8 Ionic fraction for Element VIII --- LogX9 Ionic fraction for Element IX --- LogX10 Ionic fraction for Element X --- LogX11 Ionic fraction for Element XI --- LogX12 Ionic fraction for Element XII --- LogX13 Ionic fraction for Element XIII --- LogX14 Ionic fraction for Element XIV --- LogX15 Ionic fraction for Element XV --- LogX16 Ionic fraction for Element XVI --- LogX17 Ionic fraction for Element XVII --- LogX18 Ionic fraction for Element XVIII --- LogX19 Ionic fraction for Element IXX --- LogX20 Ionic fraction for Element XX --- LogX21 Ionic fraction for Element XXI --- LogX22 Ionic fraction for Element XXII --- LogX23 Ionic fraction for Element XXIII --- LogX24 Ionic fraction for Element XXIV --- LogX25 Ionic fraction for Element XXV --- LogX26 Ionic fraction for Element XXVI --- LogX27 Ionic fraction for Element XXVII --- LogX28 Ionic fraction for Element XXVIII --- LogX29 Ionic fraction for Element XXIX --- tables.tex LaTex version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Jul 02 Pasquale Mazzotta <MAZZOTTA@axtov1.roma2.infn.it> UNKNOWN UNKNOWN In table2.dat, in rows 145 to 180, C was misprinted for N Corrections have been made on 12-Mar-1999 J_A+AS_133_403.xml YY CMi: contact or near contact system? J/A+AS/133/7 J/A+AS/133/7 V photometry of YY CMi YY CMi: contact or near contact system? P G Niarchos L Mantegazza E Poretti V Manimanis Astron. Astrophys. Suppl. Ser. 133 7 1998 1998A&AS..133....7N Binaries, eclipsing Photometry binaries: eclipsing stars: individual (YY Cmi) stars: spots New V photoelectric observations of the eclipsing system YY CMi, obtained at La Silla, Chile, and Merate Observatory, Italy, are presented. New times of minima and ephemeris based on our observations are also given. The V light curve was analysed by using the WD code to derive the geometrical and physical parameters of the system. Since no spectroscopic mass ratio is available, the q-search method was applied to yield the preliminary range of the mass ratio in order to search for the final solution. First the unspotted solution was carried out by using the unperturbed parts of the light curve and applying the DC program of the WD code. The solution was performed by assuming contact (mode 3) and semi-detached (mode 4) configuration, since no classification of the system is possible from the shape of the light curve. The solution in mode 4 does not lead to an acceptable model, since the secondary was found to be slightly overcontact. Therefore the contact solution was finally adopted. Moreover the light curve peculiarities (MaxII fainter than MaxI and excess of light around the phase 0.32) were explained by assuming a cool and a hot spot on the surface of the secondary (cooler) component. The degree of contact is very small (f=~3%) and the thermal contact is poor (T_1_-T_2_)=~650K. These results together with the high photometric mass ratio q=~0.89 indicate that YY CMi is very probably a system at the beginning or the end of the contact phase.
YY CMi HD 67110 08 06 38.5 +01 55 46 HD 66925 08 05 47.7 +02 09 54
Individual V observations of YY CMi HJD Heliocentric Julian date d {DELTA}V V magnitude difference respect with HD 66925 mag table1.tex LaTeX version of table.dat Patricia Bauer CDS 1998 May 15 Ennio Poretti <poretti@merate.mi.astro.it> J_A+AS_133_7.xml The Medicina survey of methanol masers at 6.7 GHz J/A+AS/134/115 J/A+AS/134/115 Medicina 6.7GHz methanol masers survey The Medicina survey of methanol masers at 6.7 GHz V I Slysh I E Val'tts S V Kalenskii M A Voronkov F Palagi G Tofani M Catarzi Astron. Astrophys. Suppl. Ser. 134 115 1999 1999A&AS..134..115S Masers Radial velocities Radio sources Surveys HII regions ISM: molecules masers radio lines: ISM File table2 contains the name of the sources and their coordinates (1950) observed, but not detected, with the Medicina Radiotelescope at 6.7GHz in 1995, march. Source are associated with one or more type of phenomena typical of star forming regions (see note 1 for code description). The number of non detected sources is 387.
List of undetected sources. The typical detection limit (3{sigma} level) is 3Jy. Name Name of the source --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec RV LSR radial velocity km/s Type Type of associated phenomena number=1 BO: Bipolar outflow. HII: HII region from Helfand et al. (1992ApJS...80..211H). WC: IRAS source that satisfy the Wood & Churchwell (1989ApJ...340..265W) colour criteria. other: Alternative source name. --- Patricia Bauer CDS 1998 Dec 10 Francesco Palagi <palagi@arcetri.astro.it> J_A+AS_134_115.xml Rotation in molecular clouds J/A+AS/134/241 J/A+AS/134/241 Rotation in molecular clouds Rotation in molecular clouds J P Phillips Astron. Astrophys. Suppl. Ser. 134 241 1999 1999A&AS..134..241P Morphology Nebulae Rotational velocities ISM: clouds ISM: kinematics and dynamics ISM: molecules ISM: structure We have investigated a broad range of evidence concerning rotation in molecular clouds. As a consequence, we show that trends in specific angular momentum J/M and angular velocity {Omega} are inconsistent with certain models of isothermal, non-magnetic cloud rotation. Similarly, models of rotation which invoke turbulent vorticity may have only limited applicability to clumps and condensations. There is evidence to favour an important role for rotation in maintaining the stability of disks, larger cloud structures, and perhaps a large fraction of intermediate sized clouds, whilst rotation may also be implicated in maintaining observed departures from cloud sphericity.
Rotational parameters of molecular clouds Name Name of source --- Note Notes, see file notes.txt --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec l_Dist Limit flag on Dist --- Dist Distance to cloud kpc u_Dist Uncertainty flag on Dist --- RV LSR velocity of cloud km/s DV Kinematic line width (lower value of interval when "->") km/s --- Indicates an interval --- DV2 Upper kinematic line width when interval km/s l_Size Limit flag on Size --- Size Size of cloud, over the region of maximum velocity gradient, i.e. perpendicular to the axis of rotation. (lower value when interval) pc n_Size Indicates an interval --- Size2 Upper size of cloud when interval pc Trans Molecular transition(s) employed for the observations --- L_OMEGA Limit flag on OMEGA --- OMEGA Angular rotation rate (lower value when interval) 10-14s-1 --- Indicates an interval --- OMEGA2 Upper angular rotation rate when interval 10-14s-1 l_GAMMA Limit flag on GAMMA --- GAMMA Cloud aspect ratio determined from molecular emission contours (major axis/minor axis), corresponding to the region of rotation --- l_Mass Limit flag on Mass --- Mass Cloud mass for rotating cloud, or rotating portion of cloud, determined (primarily) from column density estimates. (lower value when interval) solMass --- Indicates an interval --- Mass2 Upper cloud mass value when interval solMass MassEm Mass of embedded stars solMass THETA Orientation of rotation axis with respect to the galactic plane deg --- "->" interval; "/" two possible values --- THETA2 Upper orientation of rotation axis value if interval, or second possible value deg OMEGAo Relative orientations of the cloud minor axis, and axis of rotation Y if OMEGA is within 30{deg} of the minor axis, N otherwise. --- u_OMEGAo Uncertainty flag on OMEGAo --- Type Cloud type MI: Intermediate cloud MS: Isolated small cloud ML: Large cloud CL: Clumps MIC: Condensation within an intermediate sized cloud MLF: Filamentary large sized cloud MLC: Condensation within a large sized cloud D/R: Ring and disk MIF: Filamentary intermediate sized cloud MSFC: Condensation and filamentary within a small sized cloud --- r_Name Reference(s), see file "refs.dat" --- References of table1.dat Ref Reference number --- Aut Authors' name --- BibCode Reference in Bibcode form --- notes.txt Notes on table1.dat Patricia Bauer CDS 1998 Aug 31 Peter Phillips <jpp@udgserv.cencar.udg.mx> J_A+AS_134_241.xml The EXOSAT Medium energy Slew Survey Catalog J/A+AS/134/287 J/A+AS/134/287 EXMS catalog The EXOSAT Medium energy Slew Survey Catalog A P Reynolds A N Parmar P J Hakala A M T Pollock O R Williams A Peacock B G Taylor Astron. Astrophys. Suppl. Ser. 134 287 1999 1999A&AS..134..287R VI/43 : EXOSAT Observation Log (EXOSAT Obs 1987; Sternberg+ 1986) telnet://xray@exosat.estec.esa.nl : EXOSAT database X-ray sources Surveys We present a catalog of X-ray sources observed during slew maneuvers by the Medium Energy Detector Array onboard the EXOSAT Observatory. The EXOSAT Medium Energy slew-survey catalog (EXMS) provides a unique record of the 1-8keV X-ray sky between 1983 and 1986. 98% of the sky was observed, with 85% receiving an exposure of >60s. 1210 sources were detected. By comparing these source positions with other catalogs, identifications are given for 992 detections (82% of the sample). These identifications consist of 250 distinct objects, including 95 different X-ray binary systems, and 14 different AGN. A further 58 detections have multiple candidates, while 160 detections remain unidentified. Collimator transmission corrected 1-8keV count rates are given for the identified sources, together with raw count rates for the other detections. The construction of the EXMS and the checks performed to ensure the validity of the derived source properties are discussed. A publically available version of this catalog is maintained on the EXOSAT database and archive system (telnet://xrayxosat.estec.esa.nl).
EXOSAT Keywords: astronomical databases: miscellaneous - catalogs - X-rays: general
All singly-identified EXMS entries EXMS Object designation number=1 A designation in the form EXMS BHHMM+DDd, where HHMM and DDd are the RA and Decl. of the uncertainty region centroid in epoch 1950 coordinates. (Note: in order to maximise the usefulness of Tables 3, 4 and 5, all coordinates therein are presented for epoch 2000, although all prior catalog searches and computations were performed using epoch 1950 coordinates). Most detections have a unique EXMS classification. In cases where the classification is not unique, designators in the form (A), (B), etc are appended. In order to usefully group identifications, detections have been ordered in RA of the proposed candidate. Detections with the same coordinate (but unique designator) may be split between tables depending on the category of the identification. In cases where an identified source was observed more than once, the entries are additionally ordered by detection time. --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination (2000) --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Detec.Y Time of the detection (year) yr --- --- Detec.D Time of the detection (day) d Detec.h Time of the detection (hour) h --- --- Detec.m Time of the detection (min) min Ident Proposed identification number=2 The proposed identifications are given (truncated to 18 characters), followed by a "type" string which gives the first three letters of the catalog from which the identification was drawn (see the list of catalogs above), or the object category. The object categories are XRB: X-ray binaries SNR: supernova remnant CLU: cluster of galaxies AGN: active galactic nucleus. In this context we adopt the widest possible meaning of the term AGN, including Seyfert galaxies, BL Lacertae objects, QSOs, quasars, Radio Galaxies and Optical Violent Variables (OVVs). --- Type Proposed type number=2 The proposed identifications are given (truncated to 18 characters), followed by a "type" string which gives the first three letters of the catalog from which the identification was drawn (see the list of catalogs above), or the object category. The object categories are XRB: X-ray binaries SNR: supernova remnant CLU: cluster of galaxies AGN: active galactic nucleus. In this context we adopt the widest possible meaning of the term AGN, including Seyfert galaxies, BL Lacertae objects, QSOs, quasars, Radio Galaxies and Optical Violent Variables (OVVs). --- CountRate Collimator corrected count rate ct/s e_CountRate rms uncertainty on CountRate ct/s xi2 Chi-square of fit to the light curve number=3 Large values of reduced chi-square may indicate source variability. --- d_xi2 Number of degrees of freedom. --- lambda Parameter lambda number=4 Lambda is the likelihood detection statistic which is the difference in the logarithm of the likelihood between the best-fit and null-hypothesis models with no source present. --- F Flag values (ranging between 2 and 4) --- Dist Collimator distances number=5 Detections with collimator distances greater than about 30 arcminutes may contain large errors in their corrected count rates and should be treated with caution. arcmin Multiply identified EXMS entries EXMS Object designation --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination (2000) --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Detec.Y Time of the detection (year) yr --- --- Detec.D Time of the detection (day) d Detec.h Time of the detection (hour) h --- --- Detec.m Time of the detection (min) min Ident Proposed multiple candidates --- Type Proposed type --- CountRate Collimator corrected count rate ct/s e_CountRate rms uncertainty on CountRate ct/s xi2 Chi-square of fit to the light curve --- d_xi2 Number of degrees of freedom. --- lambda Parameter lambda --- Uncertainty regions for unidentified EXMS entries EXMS Object designation --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination (2000) --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Detec.Y Time of the detection (year) yr --- --- Detec.D Time of the detection (day) d Detec.h Time of the detection (hour) h --- --- Detec.m Time of the detection (min) min RAdeg1 First region right ascension (2000) deg DEdeg1 First region declination (2000) deg RAdeg2 Second region right ascension (2000) deg DEdeg2 Second region declination (2000) deg RAdeg3 Third region right ascension (2000) deg DEdeg3 Third region declination (2000) deg RAdeg4 Fourth region right ascension (2000) deg DEdeg4 Fourth region declination (2000) deg CountRate Collimator corrected count rate ct/s e_CountRate rms uncertainty on CountRate ct/s xi2 Chi-square of fit to the light curve --- f_xi2 Number of degrees of freedom. --- lambda Parameter lambda --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1999 Jan 04 Alastair Reynolds <areynold@estsa2.estec.esa.nl> J_A+AS_134_287.xml A Spectroscopic Study of the Themis Family J/A+AS/134/463 J/A+AS/134/463 Themis Family A Spectroscopic Study of the Themis Family M Florczak D Lazzaro T Mothe-Diniz C A Angeli A S Betzler Astron. Astrophys. Suppl. Ser. 134 463 1999 1999A&AS..134..463F Minor planets minor planets, asteroids Observational circumstances of 36 members of the Themis family observed at the 1.52m telescope of ESO (La Silla) under the agreement with the CNPq-Observatorio Nacional (Brazil). File Summary:
Observational circumstances Asteroid Asteroid number --- Name Asteroid name --- Day Previous days when observed for more than one day --- UTDate Most recent observation date "DD/MM/YY" NExp Number of expositions --- R Heliocentric distance AU DELTA Geocentric distance AU alpha Solar phase angle deg mvis Visual magnitude mag Diam Object diameter km n_Diam *: IRAS diameter --- Analog Identification of Solar Analog --- tablea1.ps PostScript version of table1 tablea1.tex TeX version of table1 Patricia Bauer CDS 1998 Sep 17 Daniela Lazzaro <lazzaro@obsn.on.br> J_A+AS_134_463.xml The Hamburg Quasar Survey. III. Further new bright quasars. J/A+AS/134/483 J/A+AS/134/483 The Hamburg Quasar Survey. III. The Hamburg Quasar Survey. III. Further new bright quasars. H -J Hagen D Engels D Reimers Astron. Astrophys. Suppl. Ser. 134 483 1999 1999A&AS..134..483H J/A+AS/128/507 : The Hamburg Quasar Survey. II. (Engels+ 1998) Hagen et al., Paper I. 1995A&AS..111..195H Magnitudes QSOs Redshifts quasars: general surveys Table 3 lists for all new QSOs the position for equinox 2000.0 with an accuracy ~2", the B magnitude obtained from the Schmidt plates with an accuracy ~<0.5 (see Paper I, Hagen et al., 1995A&AS..111..195H), the redshift, and the number of the campaign of Table 2 in which the data were obtained.
New QSOs from the Hamburg Quasar Survey Object Name Object name --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec l_Bmag Approximate flag on Bmag --- Bmag B magnitude mag z Redshift --- Run Run number --- table3.ps PostScript version of table3 table3.tex LaTeX version of table3 Patricia Bauer CDS 1998 Sep 21 H.-J. Hagen <st2b103@hs.uni-hamburg.de> J_A+AS_134_483.xml Be stars in and around young clusters in the Magellanic Clouds J/A+AS/134/489 J/A+AS/134/489 Be stars in MC young clusters Be stars in and around young clusters in the Magellanic Clouds S C Keller P R Wood M S Bessell Astron. Astrophys. Suppl. Ser. 134 489 1999 1999A&AS..134..489K J/AJ/108/932 : Variable stars in the SMC cluster NGC 330 (Sebo+, 1994) J/A+A/317/448 : BVRHalpha photometry of NGC 1818 (Grebel 1997) Clusters, open Magellanic Clouds Photometry Stars, Be galaxies: clusters: general Magellanic Clouds stars: emission-line, Be We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.
H{alpha} emission stars near NGC 1818 H{alpha} emission stars near NGC 1948 H{alpha} emission stars near NGC 2004 H{alpha} emission stars near NGC 2100 H{alpha} emission stars near NGC 330 H{alpha} emission stars near NGC 346 Name IAU designation (starting bye the cluster name) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag V-I V-I colour index mag R-Ha R-H{alpha} colour index mag Names Other names number=1 Other designations; A/B/C/D refer to Robertson, 1974A&AS...15..261R Bal to Balona, 1992MNRAS.256..425B sw to Sebo and Wood, 1994, Cat. <J/AJ/108/932> --- tables.ps PostScript version of the tables tables.tex LaTeX version of the tables Patricia Bauer CDS 1998 Nov 06 Stephan Keller <stefan@mso.anu.edu.au> J_A+AS_134_489.xml Catalogs of temperatures and [Fe/H] averages for evolved G and K stars J/A+AS/134/523 J/A+AS/134/523 Temperatures and [Fe/H] for evolved G and K stars Catalogs of temperatures and [Fe/H] averages for evolved G and K stars B J Taylor Astron. Astrophys. Suppl. Ser. 134 523 1999 1999A&AS..134..523T III/200 : Catalogue of [Fe/H] (Cayrel de Strobel+, 1997) Abundances, [Fe/H] Effective temperatures Stars, G-type Stars, K-type catalogs The catalog contains mean values of [Fe/H] (with rms errors) for 1117 evolved G-K stars. Literature references are given for the source data, which are all from high-dispersion or related work. A number of literature sources which are not used are listed with their reasons for being set aside. A FORTRAN program for listing samples from the catalog is also included. The temper.dat file contains values of Johnson V-K, {theta} [=5040/T_eff_] and E(B-V) for 346 evolved G-K stars.
The [Fe/H] catalog (with reference numbers) Name HD number or star name --- Comm Comment number (see file "comment.dat") --- Tflag Flag 'T' when a temperature exists in file "temper.dat" --- HR HR number --- [Fe/H] Mean value of [Fe/H] [Sun] e_[Fe/H] Standard deviation for mean value of [Fe/H] [Sun] nu Degrees of freedom for standard deviation --- Nref Number of references --- r_[Fe/H] Up to 14 comma-separated references (14*3 + 13 bytes) --- Comments to the catalog Comm Comment number (repeated for continuations) --- l If comment requires more than 1 line, this byte contains the total number of lines for the comment. --- Text Comment --- V-K, theta, E(B-V) Name HD number or star name --- HR HR number --- (V-K)j Johnson V-K mag e_(V-K)j Standard deviation for Johnson V-K mag theta 5040/T(eff) --- e_theta Standard deviation for theta --- E(B-V) E(B-V) mag Reference numbers, literature sources Ref Reference number --- n_Ref * if the reference number is not the number in Cayrel de Strobel et al., 1992A&AS...95..273C --- l If reference requires more than 1 line, this byte contains the total number of lines for the reference. --- BibCode Simbad Bibcode --- Text Authors name and remarks --- Unused sources (with explanations) Ref Reference number --- n_Ref * if the reference number is not the number in Cayrel de Strobel et al., 1992A&AS...95..273C --- l If reference requires more than 1 line, this byte contains the total number of lines for the reference. --- BibCode Simbad Bibcode --- Text Authors name and remarks --- Patricia Bauer CDS 1998 Sep 22 Benjamin J. Taylor <taylorb@physc1.byu.edu>, 22-Sep-1998 UNKNOWN UNKNOWN * 01-Apr-1999: The three last records of the file "catalog.dat" were updated (sign of star names) J_A+AS_134_523.xml uvby Photometry of the chemically peculiar stars. HD 15980, HR 1094, 33 Gem, and HD 115708 J/A+AS/134/53 J/A+AS/134/53 uvby photometry of 4 CP stars uvby Photometry of the chemically peculiar stars. HD 15980, HR 1094, 33 Gem, and HD 115708 S J Adelman Astron. Astrophys. Suppl. Ser. 134 53 1999 1999A&AS..134...53A J/A+AS/103/1 : 63 And, HD 192913, HR 8240 & 108 Aqr (Adelman+ 1994) J/A+AS/106/333 : Alpha And, HD 184905, HR 8216 & HR 8434 (Adelman+ 1994) J/A+AS/114/253 : HD 11187, HD 14940, HD 15144, 20 Eri, HR 8933 (Adelman+ 1995) J/A+AS/122/249 : HD 32633, 25 Sex, HR 7224 & HD 200311 (Adelman, 1997) J/A+AS/125/65 : HD 37776, HR 2258, HR 6958 & 108 Aqr (Adelman, 1997) J/PASP/109/9 : HR 1643, Theta Aur, 49 Cam, and HR 3724 (Adelman 1997) J/A+AS/125/497 : Theta Vir and 109 Vir (Adelman 1997) J/A+AS/128/245 : AR Aur, 3 Hya, 49 Cnc & BX Boo (Adelman 1997) J/A+AS/133/197 : 33 Tau, HD 50169 and HR 7786 (Adelman+ 1998) Photometry, uvby Stars, variable stars: chemically peculiar stars: individual (HD 15980, HR 1094, 33 Gem, HD 115708) Differential Stroemgren uvby photometry obtained with the Four College Automated Photoelectric Telescope shows that the hot HgMn star 33 Gem is photometrically constant. The Si star HD 15980 is found to be a variable whose period is significantly greater than 2 years. The unusual magnetic chemically peculiar Co star HR 1094 is discovered to be a low amplitude photometric variable with the magnetic field period of Hill & Blake (1996MNRAS.278..183H), 2.9761 days. The ephemeris for the magnetic chemically peculiar star HD 115708 of Wade et al. (1996A&A...307..500W) is confirmed with the error in its period of 5.07622 days being greatly reduced. The u, v, b, and y light curves for both HR 1094 and HD 115708 exhibit differences which indicate complex elemental photospheric abundance distributions.
HD 15980 02 35 13.9 +40 35 49 HR 1094 HD 22316 03 38 19.5 +56 56 00 HD 49606 33 Gem 06 49 49.8 +16 12 11 HD 115708 13 18 37.1 +26 21 56
Photometry of HD 15980 Photometry of HR 1094 (c=HD 23383, ck=HD 23594) Photometry of 33 Gem (c=HD 48907, ck=HD 47863) Photometry of HR 1094 (c=HD 21447, ck=HD 20536) </tableLink> </tableLinks> <fields> <field> <name>HJD</name> <definition>Heliocentric Julian Date</definition> <units>d</units> </field> <field> <name>u(v-c)</name> <definition>variable-comparison (v-c) u magnitude</definition> <units>mag</units> </field> <field> <name>u(ch-c)</name> <definition>check-comparison (ch-c) u magnitude</definition> <units>mag</units> </field> <field> <name>v(v-c)</name> <definition>variable-comparison (v-c) v magnitude</definition> <units>mag</units> </field> <field> <name>v(ch-c)</name> <definition>check-comparison (ch-c) v magnitude</definition> <units>mag</units> </field> <field> <name>b(v-c)</name> <definition>variable-comparison (v-c) b magnitude</definition> <units>mag</units> </field> <field> <name>b(ch-c)</name> <definition>check-comparison (ch-c) b magnitude</definition> <units>mag</units> </field> <field> <name>y(v-c)</name> <definition>variable-comparison (v-c) y magnitude</definition> <units>mag</units> </field> <field> <name>y(ch-c)</name> <definition>check-comparison (ch-c) y magnitude</definition> <units>mag</units> </field> </fields> </tableHead> <tableHead> <tableLinks> <tableLink xlink:href="tablea.dat"> <title>Yearly means and standard deviations Star Star name --- n_Star a for table4a.dat and table5a.dat data b for table4b.dat and table5b.dat data --- Per Period --- u(v-c) variable-comparison (v-c) u magnitude mag e_u(v-c) rms uncertainty on u(v-c) mag u(ch-c) check-comparison (ch-c) u magnitude mag e_u(ch-c) rms uncertainty on u(ch-c) mag v(v-c) variable-comparison (v-c) v magnitude mag e_v(v-c) rms uncertainty on v(v-c) mag v(ch-c) check-comparison (ch-c) v magnitude mag e_v(ch-c) rms uncertainty on v(ch-c) mag b(v-c) variable-comparison (v-c) b magnitude mag e_b(v-c) rms uncertainty on b(v-c) mag b(ch-c) check-comparison (ch-c) b magnitude mag e_b(ch-c) rms uncertainty on b(ch-c) mag y(v-c) variable-comparison (v-c) y magnitude mag e_y(v-c) rms uncertainty on y(v-c) mag y(ch-c) check-comparison (ch-c) y magnitude mag e_y(ch-c) rms uncertainty on y(ch-c) mag Patricia Bauer CDS 1998 Jul 15 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> J_A+AS_134_53.xml Speckle observations of double and multiple stars at Pic du Midi: measurements during 1995 and 1997 and new orbits J/A+AS/134/545 J/A+AS/134/545 Double star measurements 1995-1997 Speckle observations of double and multiple stars at Pic du Midi: measurements during 1995 and 1997 and new orbits E Aristidi J -L Prieur M Scardia L Koechlin R Avila M Carbillet B Lopez Y Rabbia P Nisenson D Gezari Astron. Astrophys. Suppl. Ser. 134 545 1999 1999A&AS..134..545A V/39 : 4th Catalog of Orbits of Visual Binaries (Worley+, 1983) Binaries, orbits Stars, double and multiple binaries: close techniques: interferometric We present speckle observations of 48 double and multiple stars observed with the 2-meter ``Telescope Bernard Lyot'' (TBL) in December 1995, January 1997 and June 1997. Angular separations, absolute position angles and relative photometry result from these observations. New orbital elements have been recalculated for 8 double stars.
Table of measurements Name WDS or HD designation --- ID Discover identified --- Mult. Number of stars of the system --- RefStar Reference star name number=1 {nu} Cyg was in fact discovered as double and then not used as reference star in the processing of BU 151 --- Epoch Epoch of observation yr lambda Wavelength nm Dlambda Band width nm ExpTime Exposition time ms n_ExpTime +: observation with the PAPA detector --- Object Name of the measured component of the multiple star number=2 For {epsilon} Hya, the angular separation ABxC was computed from AB, AC and {DELTA}m_AB_ as the distance between C and the photocenter of AB. --- Ref Latest orbit reference number=3 For orbits prior to 1982 (followed by a *), orbital elements were found in the catalog of Worley & Heintz, 1983, Cat. <V/39> --- rho Predicted separation angle arcsec e_rho rms uncertainty on rho arcsec n_rho n: not detected --- rhocal Calculated separation angle arcsec Drho rho minus rhocal arcsec theta Predicted position angle deg e_theta rms uncertainty on theta deg thetacal Calculated position angle deg Dtheta theta minus thetacal deg Dmag magnitude difference mag e_Dmag rms uncertainty on Dmag mag References BibCode BibCode --- Aut Author's name --- Com Comment --- Patricia Bauer CDS 1999 Feb 01 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_134_545.xml The central region of the Fornax cluster. I. A catalog and photometric properties of galaxies in selected CCD fields J/A+AS/134/59 J/A+AS/134/59 The central Fornax Cluster. I. Galaxy photometry The central region of the Fornax cluster. I. A catalog and photometric properties of galaxies in selected CCD fields M Hilker M Kissler-Patig T Richtler L Infante H Quintana Astron. Astrophys. Suppl. Ser. 134 59 1999 1999A&AS..134...59H VII/180 : Galaxies in 3.5 degs of Fornax cluster (Ferguson+ 1989) J/A+AS/134/75 : Paper II. Galaxy spectroscopy (Hilker+ 1999) Sersic J.-L., 1968, Atlas de galaxias australes, Observatorio Astronomica, Cordoba Clusters, galaxy Galaxies, photometry catalogs galaxies: clusters: individual (Fornax cluster) galaxies: dwarf galaxies: fundamental parameters galaxies: photometry In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. <VII/180>) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. <J/A+AS/134/75>, Paper II in this series).
Photometric catalog CGF Catalog name of the object number=1 The catalog names are prefixed by the acronym CGF (Catalog of Galaxies in Fornax) followed by a sequence number of the field and the sequence number of the galaxy in this field (ordered with decreasing magnitude). In the catalog the galaxies are ordered by increasing right ascension --- n_CGF *: objects that are also listed in appendb.dat file --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vtot Total V apparent magnitude mag nbo Neighbouring object number=2 The letter "n" indicates that a neighbouring object is present within two isophotal radii --- sbVp V peak surface brightness mag/arcsec2 V-I (V-I) color within 3 arcsec aperture mag ell Ellipticity, ell = 1 - b/a --- PA Position angle of the major axis number=3 0 degree is in east direction, positive angles towards the south, and negative angles towards the north direction deg aphot Size of the major axis arcsec d26 Size of major axis at sbV = 26 mag/arcsec2 arcsec aeff Effective semi-major axis arcsec sbVeff V effective surface brightness mag/arcsec2 Catalog of profile fit parameters CGF Catalog name of the object (see Appendix A) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec MType Morphological Type --- Vtot Total V apparent magnitude mag nbo Neighboring object (see Appendix A) --- rcap Apparent core radius number=1 Radius where the apparent central surface intensity has its half value arcsec rccor Corrected core radius (using Kormendy 1985ApJ...295...73K) arcsec sbVcor Corrected central surface brightness (sb) mag/arcsec2 nsers Exponent of Sersic (1968, Atlas de galaxias australes) profile fit --- sbVser Central surface brightness of Sersic fit mag/arcsec2 r0sers Scale length of Sersic profile fit arcsec sbVdV Central sb of de Vaucouleurs profile fit mag/arcsec2 refdV Effective radius of de Vaucouleurs profile arcsec sbVexp Central sb of exponential profile fit mag/arcsec2 alpha Scale length of exponential profile fit arcsec flag Exponential profile fit flag number=2 b: bulge is present d: light deficiency in the center n: nucleus present e: exponential law at all radii --- M. Hilker Pontifica Universidad Catolica, Santiago 1998 Jun 30 J_A+AS_134_59.xml The central region of the Fornax cluster. II. Spectroscopy and radial velocities of member and background galaxies J/A+AS/134/75 J/A+AS/134/75 Central Fornax Cluster. II. Galaxy spectroscopy The central region of the Fornax cluster. II. Spectroscopy and radial velocities of member and background galaxies M Hilker L Infante G Vieira L Infante M Kissler-Patig T Richtler Astron. Astrophys. Suppl. Ser. 134 75 1999 1999A&AS..134...75H VII/180 : Galaxies in 3.5 degs of Fornax cluster (Fergusson+ 1989) J/A+AS/134/59 : Paper I. Galaxy photometry (Hilker+ 1999) Clusters, galaxy Radial velocities galaxies: abundances galaxies: clusters: individual (Fornax cluster) galaxies: distances and redshifts galaxies: dwarf In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. <J/A+AS/134/59>). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. <VII/180>). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.
Radial velocities of galaxies CGF Catalog name of the object number=1 The catalog names are prefixed by the acronym CGF (Catalog of Galaxies in Fornax) followed by a sequence number of the field and the sequence number of the galaxy in this field (see Appendix A of Paper I, Hilker et al., 1998, Cat. <J/A+AS/134/59>). The letters "a" and "b" appended to the catalog name indicate two possible velocity determinations of the object. Three objects are prefixed by the acronym FCC (Fornax Cluster Catalog, Ferguson, 1989, Cat. <VII/180>). They are not present in our photometric catalog of Paper I, and there positions are taken from the FCC. In this table the galaxies are ordered with increasing right ascension --- Mtype Morphological type --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vtot Total V apparent magnitude mag RVcr Heliocentric velocity from cross correlation km/s Rcr R value (amplitude of cross corr. peak) --- RVrv Heliocentric velocity (task rvidlines) km/s RVem Heliocentric velocity from emission lines km/s RV Adopted heliocentric velocity km/s e_RV Mean error of different vel. determinations km/s q_RV Quality parameter of vel. determination number=2 We defined 4 classes of quality due to the clearness/evidence of the velocity identification: (1) a clear and evident identification, both velocity determination methods agree very well (2) very probable identification, almost clear (3) doubtful, but most probable value (4) very doubtful, only a try --- M. Hilker Pontifica Universidad Catolica, Santiago 1998 Jun 30 J_A+AS_134_75.xml Photographic observations of visual double stars J/A+AS/134/87 J/A+AS/134/87 Photographic observations of visual binaries Photographic observations of visual double stars D M D Jasinta M Raharto E Soegiartini Astron. Astrophys. Suppl. Ser. 134 87 1999 1999A&AS..134...87J I/211 : CCDM, Components of Double and Multiple stars (Dommanget+ 1994) I/196 : Hipparcos Input Catalogue, Version 2 (Turon+ 1993) J/A+AS/107/235 : Observations of binaries (Jasinta+ 1994) J/A+AS/114/487 : Photographic observations of visual binaries (Jasinta+ 1995) Van Albada-Van Dien E., 1983A&AS...52..193V Stars, double and multiple astrometry binaries: visual The photographic observations of 72 visual double stars are presented. The observations were made in the years 1992-1997 with the 60-cm double refractor of the Bosscha Observatory at Lembang.
Photographic observations of visual double stars CCDM CCDM (Cat. <I/211>) number --- Name Star name --- m_Name Multiplicity index in Name --- mag1 First component magnitude mag --- Separation sign --- mag2 Second component magnitude mag SType Spectral type --- Epoch Epoch of observation yr DRAcosDE Mean value of {DELTA}{alpha}cos{delta} arcsec e_DRAcosDE Standard error of DRAcosDE mas DDE Mean value of {DELTA}{delta} arcsec e_DDE Standard error of DDE mas Theta Position angle deg e_Theta Standard error of theta 0.01deg Rho Separation arcsec e_Rho Standard error of Rho mas Plates Number of plates --- Images Number of images --- Weight Weight 0.001 HIC HIC (Cat. <I/196>) numbers --- Patricia Bauer CDS 1999 Jan 14 Dini Maria Dewi Jasinta <JASINTA@sirius.as.itb.ac.id> J_A+AS_134_87.xml Mining in the Hipparcos raw data J/A+AS/135/231 J/A+AS/135/231 Mining in the Hipparcos raw data Mining in the Hipparcos raw data J L Falin F Mignard Astron. Astrophys. Suppl. Ser. 135 231 1999 1999A&AS..135..231F I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Parallaxes, trigonometric Proper motions Stars, double and multiple astrometry binaries: visual stars: fundamental parameters We give 139 reprocessed problem double stars using Hipparcos data
Stars with no Hipparcos solutions New component solutions (Stars flagged C) Hipparcos solution with time dependent proper motion (Stars flagged G) Suspected doubles (Stars flagged S, HIP<60000) Suspected doubles (Stars flagged S, HIP>60000) Stochastic solutions (Stars flagged X, HIP<60000) Stochastic solutions (Stars flagged X, HIP>60000) HIP Hipparcos identifier --- RAdeg Right ascension (ICRS, Epoch=1991.25) deg DEdeg Declination (ICRS, Epoch=1991.25) deg Plx Parallax mas pmRA Proper motion in RA (mu_alpha_*cos(delta)) mas/yr pmDE Proper motion in DE mas/yr e_RAdeg Standard error in RA mas e_DEdeg Standard error in DE mas e_Plx Standard error in Parallax mas e_pmRA Standard error in Proper motion in RA (e_mu*cos(DE)) mas/yr e_pmDE Standard error in Proper motion in DE mas/yr F1 Percentage of rejected Data % F2 Goodness-of-fit statistic number=1 Values exceeding +3 indicate a bad fit to the data. --- Source Origin of the information on the new double number=2 HIC: Hipparcos Input Catalogue, Version 2 (Turon+ 1993), Cat. <I/196> SS1: Digitalized Sky Survey first epoch SS2: Digitalized Sky Survey second epoch TYC: Tycho Catalogue (ESA 1997), Cat. <I/239> LAM: Lampens & Oblak (1998, A&A, in prep.) --- Theta Position angle relative to primary deg Sep Separation primary-secondary arcsec e_Sep Standard error of separation arcsec Dmag Difference of magnitude mag e_Dmag Standard error of Dmag mag Jean-Louis Falin OCA/CERGA Patricia Bauer CDS 1999 Jan 12 Jean-Louis Falin <falinjl@obs-azur.fr> J_A+AS_135_231.xml Gigahertz Peaked Spectrum sources from the Jodrell Bank-VLA Astrometric Survey I. Sources in the region 35{deg}<={delta}<=75{deg} J/A+AS/135/273 J/A+AS/135/273 408MHz obs. of GPS sources from JVAS survey Gigahertz Peaked Spectrum sources from the Jodrell Bank-VLA Astrometric Survey I. Sources in the region 35{deg}<={delta}<=75{deg} A Marecki H Falcke J Niezgoda S T Garrington A R Patnaik Astron. Astrophys. Suppl. Ser. 135 273 1999 1999A&AS..135..273M Radio sources catalogs galaxies: active quasars: general radio continuum: general Observations with MERLIN at 408 MHz have been used to establish the low-frequency part of the spectra of more than a hundred compact radio sources taken from the part of the Jodrell Bank-VLA Astrometric Survey (JVAS) limited by 35{deg}<={delta}<=75{deg}. These sources were selected from JVAS and other catalogues to have convex spectra between 1.4 and 8.4GHz, characteristic of Gigahertz Peaked Spectrum sources. We have confirmed convex shapes of the spectra of 76 objects.
Subsample Two - flux densities at 408 MHz IAU IAU name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec S408MHz Flux density at 408 MHz mJy Type Object type number=1 BL: BL Lac object BS: blue stellar object (without the spectrum - basically a quasar) BG: blue galaxy? CW: crowded field - too many objects for a clean identification EF: empty field G: galaxy NS: neutral stellar object (same magnitude in both E and O prints) OB: obscured field Q: quasar RS: red stellar object --- Subsample Two - sources not measured at 408 MHz IAU IAU name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Type Object type number=1 BL: BL Lac object BS: blue stellar object (without the spectrum - basically a quasar) BG: blue galaxy? CW: crowded field - too many objects for a clean identification EF: empty field G: galaxy NS: neutral stellar object (same magnitude in both E and O prints) OB: obscured field Q: quasar RS: red stellar object --- GPS sources' spectra fitting parameters Seq Sequence number on our list --- IAU IAU name --- S0 S_0_ parameter number=1 S_0_ and nu_0_ are just parameters in the formula (2): S({nu})=S_0_/(1-e^-1^)*({nu}/{nu}_0_)^k^*(1-e^-({nu}/{nu}_0_)^l-k^) mJy nu0 {nu}_0_ parameter number=1 S_0_ and nu_0_ are just parameters in the formula (2): S({nu})=S_0_/(1-e^-1^)*({nu}/{nu}_0_)^k^*(1-e^-({nu}/{nu}_0_)^l-k^) GHz k Spectral index of the rising part --- l Spectral index of the declining part --- Smax Flux density at the maximum mJy numax Frequency of the maximum flux density GHz Flag Note number=2 We fitted the so called broken power-law to our spectra - see formula (2) in the paper. Even though it seems to be the physically more sensible choice for a model spectrum compared to a simple second-order polynomial, it has the disadvantage that it is unconstrained if the peak of the spectrum falls beyond the 2nd highest or below the 2nd lowest available frequency. In these cases we fixed the peak of the model spectrum (i.e. Smax and numax) at the peak of the measured data - this was usually the measurement at 4.85GHz - and marked the fit as "unconstrained" by putting a "+" sign in col. 61. --- Patricia Bauer CDS 1999 Mar 02 Andrzej Marecki <amr@astro.uni.torun.pl> J_A+AS_135_273.xml New periods of variable stars in Cygnus based on a quarter of century of photographic observations. J/A+AS/135/29 J/A+AS/135/29 New periods of variable stars in Cygnus New periods of variable stars in Cygnus based on a quarter of century of photographic observations. L Hric R Galis Astron. Astrophys. Suppl. Ser. 135 29 1999 1999A&AS..135...29H Magnitudes Stars, variable stars: variables: general techniques: photometric The Table2 summarizes the photographic magnitudes obtained over 24 years at the Skalnate Pleso (1979-1993) and Asiago (1969-1988) observatories for 17 variable stars of different types: Miras (7), Semi-regular (4), Cepheids (3), RR Lyr (2), Eclipsing binary (1). The cross-reference between star No., designation according to Margoni and Stagni (1984A&AS...56...87M) and catalogue one (provided it has already been adopted for a given star) according to the GCVS (See Cat. <II/214>) and IBVS (Kholopov al., 1987, See Cat. <II/195>) is given in Table3 as well as the equatorial coordinates for the epoch 1950.0 for each star, which is compatible with the GCVS. In this table are shown the basic characteristics of the observational material for each star: the number of data points and interval of magnitudes obtained at the Asiago Observatory (A) and Skalnate Pleso Observatory (SP) respectively.
Photographic magnitudes for 17 variables JD Date d No1 Magnitude for star No.1 mag No2 Magnitude for star No.2 mag No3 Magnitude for star No.3 mag No4 Magnitude for star No.4 mag No5 Magnitude for star No.5 mag No6 Magnitude for star No.6 mag No7 Magnitude for star No.7 mag No8 Magnitude for star No.8 mag No9 Magnitude for star No.9 mag No10 Magnitude for star No.10 mag No11 Magnitude for star No.11 mag No12 Magnitude for star No.12 mag No13 Magnitude for star No.13 mag No14 Magnitude for star No.14 mag No15 Magnitude for star No.15 mag No16 Magnitude for star No.16 mag No17 Magnitude for star No.17 mag Obs Observatory; See Note number=1 A : Asiago Observatory SP: Skalnate Pleso Observatory --- The basic characteristics of investigated stars No Star No. --- [MS84] Margoni and Stagni (1984A&AS...56...87M) designation --- Name GCVS/IBVS designation --- RAh Right ascension 1950 (hours) h RAm Right ascension 1950 (minutes) min RAs Right ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (arcminutes) arcmin NobsA Number of observations (Asiago Obs.) --- maxA Maximal brightness (Asiago Obs.) mag minA Minimal brightness (Asiago Obs.) mag NobsSP Number of observations (Skalnate Pleso Obs.) --- maxSP Maximal brightness (Skalnate Pleso Obs.) mag minSP Minimal brightness (Skalnate Pleso Obs.) mag Patricia Bauer CDS 1998 Dec 03 Ladislav Hric <hric@ta3.sk> J_A+AS_135_29.xml The ROSAT all-sky survey catalogue of the nearby stars J/A+AS/135/319 J/A+AS/135/319 ROSAT data of Nearby Stars The ROSAT all-sky survey catalogue of the nearby stars M Huensch J H M M Schmitt M F Sterzik W Voges Astron. Astrophys. Suppl. Ser. 135 319 1999 1999A&AS..135..319H V/70 : Nearby Stars, Preliminary 3rd Version (Gliese+ 1991) IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1996) J/A+AS/127/251 : Giants and supergiants ROSAT data (Huensch+ 1998) J/A+AS/132/155 : Main-sequence and subgiants ROSAT data (Huensch+ 1998) Stars, late-type Stars, nearby X-ray sources stars: activity stars: coronae stars: late-type X-rays: stars We present X-ray data for all entries of the Third Catalogue of Nearby Stars (Gliese and Jahreiss, 1991, Cat. <V/70>) that have been detected as X-ray sources in the ROSAT all-sky survey. The catalogue contains 1252 entries yielding an average detection rate of 32.9 percent. In addition to count rates, source detection parameters, hardness ratios, and X-ray fluxes we also list X-ray luminosities derived from Hipparcos parallaxes.
ROSAT
RASS detections of the Gliese stars Name Gliese catalogue or other designation --- Vmag V magnitude mag B-V B-V colour index mag SpType Spectral classification --- Dist Hipparcos distance pc ExpTime Exposure time s CtRate Mean PSPC count rate ct/s e_CtRate Error of PSPC count rate ct/s LH Likelihood of existence --- DO-X Offset between optical and X-ray position arcsec HR Hardness Ratio = (H-S)/(H+S) --- u_HR Uncertainty flag on HR --- e_HR Error of Hardness Ratio --- FXray Apparent X-ray flux (0.1-2.4 keV) 10-14mW/m2 u_FXray Uncertainty flag on FXray --- LXray X-ray luminosity 10+20W u_LXray Uncertainty flag on LXray --- Patricia Bauer CDS 1998 Nov 23 Matthias Huensch <supas106@astrophysik.uni-kiel.de> J_A+AS_135_319.xml Atomic data from the Iron Project XXXV. Relativistic fine structure oscillator strengths for Fe XXIV and Fe XXV J/A+AS/135/347 J/A+AS/135/347 IRON Project XXXV. Fe XXIV and Fe XXV Atomic data from the Iron Project XXXV. Relativistic fine structure oscillator strengths for Fe XXIV and Fe XXV S N Nahar A K Pradhan Astron. Astrophys. Suppl. Ser. 135 347 1999 1999A&AS..135..347N J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions NEW TABLES (12-Nov-1998) J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III NEW TABLES (12-Nov-1998) J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions J/A+AS/123/159 : IRON Project XXII. C and O radiative rates J/A+AS/123/575 : IRON Project XXIII. Fe XXII excitation rate coefficients J/A+AS/126/373 : IRON Project XXVII. Fe IV collision strengths J/A+AS/131/499 : IRON Project XXIX. Boron isoelectronic sequence J/A+AS/131/153 : IRON Project XXXI. Fe XII electron excitation 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths 1997A&AS..122..167B : IRON Project XX. Fe I oscillator strengths 1997A&AS..122..177P : IRON Project XXI. Fe I fine-structure transition 1997A&AS..126..105B : IRON Project XXIV. Fe XXIV electron excitation 1998A&AS..127..545B : IRON Project XXV. Fe XII electron excitation 1997A&AS..126..365B : IRON Project XXVI. Fe IV oscillator strengths 1998A&AS..129..161B : IRON Project XXVIII. F-like ions fine-structure trans. 1999A&AS..134..369S : IRON Project XXX. P III, S IV & Cl V collision data 1998A&AS..133..245G : IRON Project XXXII. Ar III effective collision strength 1999A&AS..135..159M : IRON Project XXXIII. Carbon radiative rates Atomic physics atomic data X-rays: galaxies The first large-scale calculations of relativistic radiative transition probabilities from the Iron Project is reported for dipole allowed and intercombination (E1) transitions in Li-like Fe XXIV and He-like Fe XXV. The ab intio calculations are carried out in the close coupling approximation using the Breit-Pauli R-matrix method in intermediate coupling characterized by SLJ, with total (2S+1)=2,4, L=7, J=1/2-11/2 even and odd parity, for Fe XXIV, and with total (2S+1)=1,3, L=9, and J=0-4 for Fe XXV. The eigenfunction expansions for the target ions include 13 levels up to the n=3 for Fe XXV, and 16 levels up to the n=4 for Fe XXVI, respectively. The calculated number of bound levels, 83 for Fe XXIV and 138 for Fe XXV, is much larger than experimentally observed. The level energies are in good agreement for the common levels. All dipole and intercombination fine structure transitions involving the calculated bound levels up to n=10 and l=5 or 6 are considered. Oscillator strengths, line strengths, and Einstein A-coefficients are tabulated for 802 transitions in Fe XXIV and 2579 transitions in Fe XXV. The results compare well with limited subsets of transitions considered in previous works including fully relativistic and QED corrections. Additional comparisons between the length and the velocity formulations indicate an overall accuracy between 1-10%. The range of uncertainty is indicative of the relatively small influence of atomic effects, such as the two-body Breit interaction terms and finite nuclear mass term, that are not included in the Breit-Pauli approximation employed in the present calculations. The extensive set of data is expected to be useful in the analysis of X-ray and XUV spectra from astrophysical sources.
*Fe XXIV target states and energies *Fe XXV target states and energies Index Level index --- Conf Electronic configuration --- Term Electronic term --- J Total angular momentum --- E Theoretical energy Ry Fe XXIV energy levels Fe XXV energy levels Index Level index --- Level Level --- J Total angular momentum --- Parity o: odd; e: even --- E Theoretical energy Ry Fe XXIV transition probabilities Fe XXV transition probabilities Conf Configuration --- Tf Total number of line for the configuration --- i Initial level --- k Final level --- gi Lande factor (2I+1) of initial state --- gk Lande factor (2J+1) of final state --- Aki Transition probability s-1 fik Oscillator strength --- S Line strength (atomic units) --- Patricia Bauer CDS 1998 Oct 22 Sultana Nahar <nahar@astronomy.ohio-state.edu> J_A+AS_135_347.xml Recombination line intensities for hydrogenic ions: the fine structure components of HI and HeII J/A+AS/135/359 J/A+AS/135/359 HI and HeII fine structure components Recombination line intensities for hydrogenic ions: the fine structure components of HI and HeII R E S Clegg S Miller P J Storey R Kisielius Astron. Astrophys. Suppl. Ser. 135 359 1999 1999A&AS..135..359C VI/64 : Recombination line intensities for hydrogenic ions (Storey+ 1995) Atomic physics atomic data HII regions line: formation line: profiles planetary nebulae: general Emissivities have been calculated for fine-structure components of selected UV and optical recombination lines of HI and HeII. Results are given for a range of electron temperatures and densities, and in Cases A and B of Baker & Menzel (1938ApJ....88...52B). Relative intensities, wavelengths and velocity shifts of the fine-structure components are tabulated. Applications to the spectra of gaseous nebulae are discussed. Depending on the temperature, density and Case, the centres of unresolved lines can shift by up to 0.9km/s for HI and 3.3km/s for HeII. A new calibration of the H{alpha}-NII method for determining electron temperatures is given.
Summary of components, and the reference wavelengths of hydrogenic transitions nu Upper state principal quantum number --- nl Lower state principal quantum number --- Nc Number of components --- D(v)HI Total range in velocity space of components for HI lines km/s D(v)HeII Total range in velocity space of components for HeII lines km/s 1HI Reference wavelength for ^1^HI 0.1nm 2HI Reference wavelength for ^2^HI 0.1nm 3HeII Reference wavelength for ^3^HeII 0.1nm 4HeII Reference wavelength for ^4^HeII 0.1nm Fine structure components for n-2 transitions Fine structure components for n-3 transitions Index Index of transition --- Stateu Upper state nl in spectroscopic notation --- Su 2S+1 of upper state term --- Lu L (spectroscopic) of upper state term --- Pu Parity (0 for even, 1 for odd) of upper state term --- Ju J of upper state term --- Statel Lower state nl in spectroscopic notation --- Sl 2S+1 of lower state term --- Ll L (spectroscopic) of lower state term --- Pl Parity (0 for even, 1 for odd) of lower state term --- Jl J of lower state term --- lu Orbital quantum number l of upper state --- 2ju Double total quantum number 2j of upper state --- ll Orbital quantum number l of lower state --- 2jl Double total quantum number 2j of lower state --- Normalized component intensities Comp Component number=1 H{alpha}: H3-2, reference wavelength 6562.8812{AA} H{beta}: H4-2, reference wavelength 4861.3784{AA} H{gamma}: H5-2, reference wavelength 4340.5086{AA} He II: He3-2, reference wavelength 1640.5055{AA} He4-2, reference wavelength 1215.1893{AA} He4-3, reference wavelength 4685.8471{AA} He5-3, reference wavelength 3203.1867{AA} --- Case Baker & Menzel (1938ApJ....88...52B) case --- Ne Electron densityI cm-3 Index Transition indeX --- D(lambda) Shift in wavelength 0.1nm D(v) Shift in velocity km/s T=300 Normalized component intensity at Te=300K --- T=1000 Normalized component intensity at Te=1000K --- T=3000 Normalized component intensity at Te=3000K --- T=10000 Normalized component intensity at Te=10000K --- T=30000 Normalized component intensity at Te=30000K --- Line emissivities Comp Component --- Case Baker & Menzel (1938ApJ....88...52B) case --- nu Upper state principal quantum number --- --- --- nl Lower state principal quantum number --- Ne Electron density cm-3 T=300 Line emissivity at Te=300K mW/m2/cm T=1000 Line emissivity at Te=1000K mW/m2/cm T=3000 Line emissivity at Te=3000K mW/m2/cm T=10000 Line emissivity at Te=10000K mW/m2/cm T=30000 Line emissivity at Te=30000K mW/m2/cm Line centre positions Comp Component --- Case Baker & Menzel (1938ApJ....88...52B) case --- nu Upper state principal quantum number --- --- --- nl Lower state principal quantum number --- Ne Electron density cm-3 T=300 Line centre positions at Te=300K 0.1nm T=1000 Line centre positions at Te=1000K 0.1nm T=3000 Line centre positions at Te=3000K 0.1nm T=10000 Line centre positions at Te=10000K 0.1nm T=30000 Line centre positions at Te=30000K 0.1nm H{alpha} full line widths and broadening terms {delta} vbroad Full line width at half maximum excluding fine-structure effects km/s FWHM Full line width at half maximum including fine-structure effects km/s delta Broadening term {delta} km/s Patricia Bauer CDS 1998 Nov 17 Romas Kisielius <rk@aura.phys.ucl.ac.uk> J_A+AS_135_359.xml VI CCD photometry of metal-rich bulge globular clusters: NGC 6553 J/A+AS/135/391 J/A+AS/135/391 VI CCD photometry of NGC 6553 VI CCD photometry of metal-rich bulge globular clusters: NGC 6553 R Sagar A Subramaniam T Richtler R K Grebel Astron. Astrophys. Suppl. Ser. 135 391 1999 1999A&AS..135..391S J/A+A/331/70 : JKVI photometry of NGC 6553 stars (Guarnieri+ 1998) Clusters, globular Photometry, CCD Galaxy: abundances globular clusters: individual (NGC 6553) stars: abundances stars: horizontal-branch stars: late-type X, Y pixel coordinates and V, I CCD photometric magnitudes of stars in cluster region NGC 6553. DAOPHOT photometric errors in V and (V-I) are also given.
NGC 6553 18 09 15.6 -25 54 28
Data of 40170 stars in NGC 6553 Seq Sequential number --- xpos x coordinate along East direction number=1 1 pixel = 0.332 arcsec pix ypos y coordinate along North direction number=1 1 pixel = 0.332 arcsec pix Vmag V magnitude mag e_Vmag Error in Vmag mag V-I V-I colour index mag e_V-I Error in V-I mag Patricia Bauer CDS 1998 Dec 14 Ram Sagar <sagar@upso.ernet.in> J_A+AS_135_391.xml Grids of stellar models. VIII. From 0.4 to 1.0 M_Sun_ at Z=0.020 and Z=0.001, with the MHD equation of state J/A+AS/135/405 J/A+AS/135/405 Grids of stellar models. VIII. Grids of stellar models. VIII. From 0.4 to 1.0 M_Sun_ at Z=0.020 and Z=0.001, with the MHD equation of state C Charbonnel W Dappen D Schaerer P A Bernasconi A Maeder G Meynet N Mowlavi Astron. Astrophys. Suppl. Ser. 135 405 1999 1999A&AS..135..405C J/A+AS/96/269 : Paper I. 0.8 to 120 M_{sun}_, Z=0.020 (Schaller+, 1992) J/A+AS/98/523 : Paper II. 0.8 to 120 M_{sun}_, Z=0.008 (Schaerer+ 1993) J/A+AS/101/415 : Paper III. 0.8 to 120 M_{sun}_, Z=0.004 (Charbonnel+ 1993) J/A+AS/102/339 : Paper IV. 0.8 to 120 M_{sun}_, Z=0.040 (Schaerer+, 1993) J/A+AS/103/97 : Paper V. 12 to 120 M_{sun}_, Z=0.001, 0.004, 0.008, 0.020 0.040 (Meynet+ 1994) J/A+AS/115/339 : Paper VI. HB abd AGB, Z=0.020, 0.001 (Charbonnel+, 1996) J/A+AS/128/471 : Paper VII. 0.8 to 60M_{sun}_, Z=0.10 (Mowlavi+ 1998) HR diagrams Mass loss Models, evolutionary Hertzsprung-Russell (HR diagram) stars: evolution stars: interiors stars: low-mass, brown dwarfs We present stellar evolutionary models covering the mass range from 0.4 to 1M_{sun}_ calculated for metallicities Z=0.020 and 0.001 with the MHD equation of state (Hummer & Mihalas, 1988ApJ...331..773H, Mihalas et al., 1988ApJ...331..815M, Daeppen et al., 1988ApJ...332..261D). A parallel calculation using the OPAL (Rogers et al., 1996ApJ...456..902R) equation of state has been made to demonstrate the adequacy of the MHD equation of state in the range of 1.0 to 0.8M_{sun}_ (the lower end of the OPAL tables). Below, down to 0.4M_{sun}_, we have justified the use of the MHD equation of state by theoretical arguments and the findings of Chabrier & Baraffe (1997A&A...327.1039C). We use the radiative opacities by Iglesias & Rogers (1996ApJ...464..943I), completed with the atomic and molecular opacities by Alexander & Fergusson (1994ApJ...437..879A). We follow the evolution from the Hayashi fully convective configuration up to the redgiant tip for the most massive stars, and up to an age of 20Gyr for the less massive ones. We compare our solar-metallicity models with recent models computed by other groups and with observations.
0.4M, Z=0.001, Y=0.243, without overshooting 0.5M, Z=0.001, Y=0.243, without overshooting 0.6M, Z=0.001, Y=0.243, without overshooting 0.7M, Z=0.001, Y=0.243, without overshooting 0.8M, Z=0.001, Y=0.243, without overshooting 0.9M, Z=0.001, Y=0.243, without overshooting 1.0M, Z=0.001, Y=0.243, without overshooting 0.4M, Z=0.020, Y=0.300, without overshooting 0.5M, Z=0.020, Y=0.300, without overshooting 0.6M, Z=0.020, Y=0.300, without overshooting 0.7M, Z=0.020, Y=0.300, without overshooting 0.8M, Z=0.020, Y=0.300, without overshooting 0.9M, Z=0.020, Y=0.300, without overshooting 1.0M, Z=0.020, Y=0.300, without overshooting 0.4M, Z=0.020, Y=0.280, without overshooting 0.5M, Z=0.020, Y=0.280, without overshooting 0.6M, Z=0.020, Y=0.280, without overshooting 0.7M, Z=0.020, Y=0.280, without overshooting 0.8M, Z=0.020, Y=0.280, without overshooting 0.9M, Z=0.020, Y=0.280, without overshooting 1.0M, Z=0.020, Y=0.280, without overshooting Npoint Number of selected point --- Age Age yr Mass Actual mass solMass log(L) log(luminosity) [solLum] log(Teff) log(effective temperature) [K] Hs H surface abundance (mass fraction) --- Hes He surface abundance (mass fraction) --- 12Cs 12C surface abundance (mass fraction) --- 13Cs 13C surface abundance (mass fraction) --- 14Ns 14N surface abundance (mass fraction) --- 16Os 16O surface abundance (mass fraction) --- 17Os 17O surface abundance (mass fraction) --- 18Os 18O surface abundance (mass fraction) --- 20Nes 20Ne surface abundance (mass fraction) --- 22Nes 22Ne surface abundance (mass fraction) --- QCC Core mass fraction --- Mdot log(mass loss rate) solMass/yr rhoc log(central density) [g/cm3] log(Tc) log(central temperature) [K] Hc H central abundance (mass fraction) --- Hec He central abundance (mass fraction) --- 12Cc 12C central abundance (mass fraction) --- 13Cc 13C central abundance (mass fraction) --- 14Nc 14N central abundance (mass fraction) --- 16Oc 16O central abundance (mass fraction) --- 17Oc 17O central abundance (mass fraction) --- 18Oc 18O central abundance (mass fraction) --- 20Nec 20Ne central abundance (mass fraction) --- 22Nec 22Ne central abundance (mass fraction) --- Patricia Bauer CDS 1998 Dec 14 Corinne Charbonnel <corinne.charbonnel@ast.obs-mip.fr> UNKNOWN UNKNOWN Pre-main sequence tracks can be asked to Corinne.Charbonnel@obs-mip.fr J_A+AS_135_405.xml AGNs with composite spectra. II. Additional data. J/A+AS/135/437 J/A+AS/135/437 AGNs with composite spectra. II. AGNs with composite spectra. II. Additional data. A C Goncalves M -P Veron-Cetty P Veron Astron. Astrophys. Suppl. Ser. 135 437 1999 1999A&AS..135..437G Active gal. nuclei Galaxies, Seyfert Galaxies, spectra H II regions Line Profiles Spectroscopy galaxies: active galaxies: nuclei galaxies: Seyfert We have compiled from the literature 88 emission-line galaxies for which the published line-ratios give indication of a "transition spectrum"; selected objects are located north of {delta}~-20{deg}, are brighter than B=17 and have z<0.1. We have observed 53 of these galaxies with the spectrograph CARELEC, attached to the OHP 1.93m telescope. The observations were carried out during several runs in May, June and July 1996 and January, March, October and November 1997. The journal of observations is given in Table 5. The spectra (R~1800) were analysed in terms of Gaussians to search for the presence of multiple line-components, coming from kinematically and spatially distinct regions - "composite spectra". The results of the fitting analysis are given in Table 6.
Journal of observations Name Galaxy name --- n_Name Note on Name number=1 *: objects published in Paper I (1997A&A...319...52V) --- Disp Dispersion & wavelength range number=2 A: observations in the range 670.0-760.0nm, R~1800 B: observations in the range 486.0-576.0nm, R~1800 --- Date Date of exposure "DD/MM/YY" ExpTime Exposure time min PA Slit position angle deg Fitting analysis results Name Galaxy name & notes on the object number=1 When several slices were extracted from the spectrum of a single object, these were numbered #1, #2, #3 etc. --- n_Name Note on Name number=2 a: an absorption feature was included in the model to fit the blue spectrum b: we added an absorption line to fit the red spectrum t: we corrected the blue spectrum for the stellar contribution by using a template q: the red spectrum was corrected by a template. --- z Redshift used in the fitting analysis --- Vblue Line velocity in the blue system km/s n_Vblue Note on the V_blue_ parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- l_FWHMblue Limit flag on FWHMblue parameter --- FWHMblue FWHM of the lines in the blue system km/s n_FWHMblue Note on the FWHMblue parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- l_5007/Hb Limt flag on the [OIII]5007/Hb parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- 5007/Hb Ratio of [OIII]5007 to the H{beta} line --- n_5007/Hb Note on the [OIII]5007/Hb parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- Hb Flux of the H{beta} line % Vred Line velocity in the red system km/s n_Vred Note on the Vred parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- l_FWHMred Limit flag on the FWHMred parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- FWHMred FWHM of the lines in the red system km/s n_FWHMred Note on the FWHMred parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- 6583/Ha Ratio of [NII]6583 to the H{alpha} line --- n_6583/Ha Note on the [NII]6583/Ha parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- l_6300/Ha Limit flag on the [NII]6583/Ha parameter number=3 *: the value on the previous column was fixed in the model. !: profile used to fit the line is Lorentzian, rather than Gaussian. --- 6300/Ha Ratio of [OI]6300 to the H{alpha} line --- Ha Flux of the H{alpha} line % DeltaV Difference between Vblue and Vred km/s Class Classification of the line-components number=4 1: Seyfert 1 2: Seyfert 2 H: H II region L: LINER --- A.C. Goncalves OHP Patricia Bauer CDS 1999 Feb 01 Anabela Goncalves <anabela@obs-hp.fr> J_A+AS_135_437.xml Variable central stars of young Planetary Nebulae. A photometric study of the central star of M2-54 J/A+AS/135/493 J/A+AS/135/493 V light curves of PN M2-54 Variable central stars of young Planetary Nebulae. A photometric study of the central star of M2-54 G Handler Astron. Astrophys. Suppl. Ser. 135 493 1999 1999A&AS..135..493H Magnitudes Planetary nebulae planetary nebulae: individual (M2-54) stars: mass-loss stars: oscillations stars: variables: other The time-series V-filter photometry of the variable central star of the Planetary Nebula M2-54 is presented.
PN M 2-54 PK 104-06 1 PN G104.8-06.7 22 51 38.8 +51 50 41
Time-series photometry of M2-54 HJD Heliocentric Julian Date d DVmag V magnitude difference M2-54 minus comp. star mag Patricia Bauer CDS 1998 Nov 20 Gerald Handler <gerald@procyon.astro.univie.ac.at> J_A+AS_135_493.xml CCD measurements of visual double stars made with the 50 cm refractor of the Nice Observatory. J/A+AS/135/499 J/A+AS/135/499 Double star measurements CCD measurements of visual double stars made with the 50 cm refractor of the Nice Observatory. M Salaman G Morlet R Gili et Astron. Astrophys. Suppl. Ser. 135 499 1999 1999A&AS..135..499S I/211 : CCDM, Components of Double and Multiple stars (Dommanget+ 1994) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) J/A+AS/102/643 : Mesure d'etoiles doubles (Muller, 1993) J/A+AS/106/377 : Double star measurements (Couteau+, 1994) J/A+AS/115/59 : Double stars measurements at Nice Obs. (Thorel+, 1996) J/A+AS/126/1 : Double stars measurements (Gili+ 1997) Stars, double and multiple astrometry binaries: visual We present the measurements of 49 visual double stars made in 1997 with the 50 cm refractor of the Nice Observatory (Table 1). A CCD camera was attached to this refractor. Some new binaries discovered by Hipparcos have been measured. The algorithm used for these measurements is based on the adjustment of a tridimensional mathematical surface.
CCD measurements of visual double stars made with the 50 cm refractor of the Nice Observatory CCDM CCDM (Cat. <I/211>) number --- Name Name of the couple number=1 HDS: star determined double by Hipparcos observations and previously unknown as double. --- m_Name Multiplicity index on Name --- HIP HIP (Cat. <I/239>) number --- mag1 Magnitude of the first component mag mag2 Magnitude of the second component mag ObsDate Observation date (in decimal years) yr PA Position angle deg Sep Separation angle arcsec Dmag Magnitude difference, measured without filters mag Nights Number of nights --- Nimage Number of images --- Patricia Bauer CDS 1999 Feb 26 Guy Morlet <gmorlet@cybercable.fr> J_A+AS_135_499.xml Radial velocities of Hipparcos southern B8-F2 type stars J/A+AS/135/503 J/A+AS/135/503 Hipparcos southern B8-F2 stars radial velocities Radial velocities of Hipparcos southern B8-F2 type stars S Grenier R Burnage R Farraggiana M Gerbaldi F Delmas A E Gomez V Sabas L Sharif Astron. Astrophys. Suppl. Ser. 135 503 1999 1999A&AS..135..503G I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Binaries, spectroscopic Radial velocities Stars, early-type galaxies: compact galaxies: distances and redshifts galaxies: fundamental parameters galaxies: starburst surveys Radial velocities have been determined for a sample of B8-F2 type stars observed by the Hipparcos satellite. Observations were obtained within the framework of an ESO key-program. Radial velocities have been measured using a cross-correlation method, the templates being a grid of synthetic spectra. The obtained precision depends on effective temperature and projected rotational velocity of the star as well as on a possible asymmetry of the correlation peak generally due to secondary components. New spectroscopic binaries have been detected from these a symmetries and the variability of the measured radial velocity. Simulations of binary and triple systems have been performed. For binaries our results have been compared with Hipparcos binary data. Adding the variable radial velocities, the minimum binary fraction has been found 60% for physical systems. Radial velocities have been determined for 581 B8-F2 stars, 159 being new. Taking into account published radial velocities, 39% south A-type stars with V magnitude lower than 7.5 have a radial velocity.
Hipparcos
Notes about peculiar and multiple stars HIP HIP (Cat. <I/239>) number --- HD HD (Cat. <III/135>) number --- m_HD Multiplicity index on HD --- Note Text of the note --- r_Note References number=1 1: Paunzen et al., 1997, Cat. <J/A+AS/123/93> 2: Gray et al., 1997 3: Abt & Morell, 1995, Cat. <J/ApJS/99/135> blank: Tokovinin, 1997, Cat. <J/A+AS/124/75> --- Individual radial velocities HIP HIP (Cat. <I/239>) number --- m_HIP Multiplicity index on HIP --- HD HD (Cat. <III/135>) number --- m_HD Multiplicity index on HD --- HJD Heliocentric Julian Day d RV Radial velocity km/s e_RV Error on RV from the equation given in section 3.1 km/s Teff Effective temperature of the synthetic spectrum K Rot Rotation broadening of the synthetic spectrum km/s Dg-p Difference between gaussian and parabolic fitting km/s Mean radial velocities and others parameters HIP HIP (Cat. <I/239>) number --- m_HIP Multiplicity index on HIP --- HD HD (Cat. <III/135>) number --- m_HD Multiplicity index on HD --- RAh Right ascension (J2000) number=1 In the original table, HIP 17797B, HIP 43920B and HIP 46657B have no positions. For HIP 17797B and HIP 46657B, we added the Simbad coordinates of the corresponding HD star. For HIP 43920B, we added the coordinates of HIP 43920A of this table. h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag Magnitude V mag Source Source of magnitude number=2 The source is G = ground-based, H=HIP, T=Tycho --- SpType Spectral type --- RV Mean radial velocity km/s e_RV rms on radial velocity when o_RV > 1 km/s ErrRV Error on radial velocity when o_RV > 1 km/s o_RV Number of observations --- eInt Mean adopted internal error km/s E/I Ratio E/I of external to internal error --- Var Variability indication --- Shape Flag on the shape of the correlation peak number=3 0: symmetric and gaussian peak 1: SB2 2: certain double, near spectral types 3: certain double, A-B type with faint F-G component 4: probable double 5: suspected double 6: probable multiple system 7: certain shell star 8: suspected shell star 9: wide and irregular peak 10: wide peak of B star (few lines) --- Note Note on the star in the table6.dat --- HvarType variability type number=4 Hipparcos-defined type of variability (a blank entry signifies that the entry could not be classified as variable or constant): D: duplicity-induced variability --- Ncomp Number of components in this entry --- MultFlag Double/Multiple Systems flag number=5 indicates that further details are given in the Double and Multiple Systems Annex: C: solutions for the components G: acceleration or higher order terms O: orbital solutions V: variability-induced movers (apparent motion arises from variability) X: stochastic solution (probably astrometric binaries with short period) --- Qual Solution quality number=6 Reliability of the double or multiple star solution: A=good, B=fair, C=poor, D=uncertain, S=suspected non-single --- HIPcomp Component identifiers --- rho Angular separation between components arcsec dHp Magnitude difference of components mag Flag * when rho and dHp are from CCDM (Dommanget & Nys, 1994, Cat. <I/211>) --- Stars with two measured peaks HIP HIP (Cat. <I/239>) number --- m_HIP Multiplicity index on HIP --- HD HD (Cat. <III/135>) number --- m_HD Multiplicity index on HD --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag Magnitude V mag Source Source of magnitude number=1 The source is G = ground-based, H=HIP, T=Tycho --- SpType Spectral type --- Shape Flag on the shape of the correlation peak (see table 4) --- Note Note on the star in the table 6 --- HvarType variability type number=2 Hipparcos-defined type of variability (a blank entry signifies that the entry could not be classified as variable or constant): D: duplicity-induced variability --- Ncomp Number of components in this entry --- MultFlag Double/Multiple Systems flag number=3 indicates that further details are given in the Double and Multiple Systems Annex: C: solutions for the components G: acceleration or higher order terms O: orbital solutions V: variability-induced movers (apparent motion arises from variability) X: stochastic solution (probably astrometric binaries with short period) --- Qual Solution quality number=4 Reliability of the double or multiple star solution: A=good, B=fair, C=poor, D=uncertain, S=suspected non-single --- HIPcomp Component identifiers --- rho Angular separation between components arcsec dHp Magnitude difference of components mag Flag * when rho and dHp are from CCDM (Dommanget & Nys, 1994, Cat. <I/211>) --- Patricia Bauer CDS 1998 Nov 24 Suzanne Grenier <grenier@mehipp.obspm.fr> J_A+AS_135_503.xml The Hamburg/SAO Survey for Emission-Line Galaxies. I. A First List of 70 Galaxies. J/A+AS/135/511 J/A+AS/135/511 The Hamburg/SAO Survey for ELGs The Hamburg/SAO Survey for Emission-Line Galaxies. I. A First List of 70 Galaxies. A V Ugryumov D Engels V A Lipovetsky H -J Hagen U Hopp S A Pustilnik A Yu Kniazev G Richter Yu I Izotov C C Popescu Astron. Astrophys. Suppl. Ser. 135 511 1999 1999A&AS..135..511U J/MNRAS/246/433 : CCD photometry + APM parameters for galaxies (Maddox+ 1990) J/A+AS/115/235 : The Hamburg/ESO survey for bright QSOs. II. (Reimers+, 1996) J/A+AS/128/507 : The Hamburg Quasar Survey. II. (Engels+ 1998) Galaxies, spectra Magnitudes Radial velocities Redshifts galaxies: compact galaxies: distances and redshifts galaxies: fundamental parameters galaxies: starburst surveys We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.
Coordinates, velocities, magnitudes and classification of emission-line galaxies Name Name of objects --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec HRV Heliocentric radial velocity km/s n_Bmag *: Magnitudes are taken from the APM, Maddox et al., Cat. <J/MNRAS/246/433> --- Bmag Magnitude in B filter mag BMAG Absolute B-magnitude mag Type Classification number=1 Only rough classification were done due to low S/N spectra. Spectral classification follows Salzer et al., 1989ApJS...70..479S --- Names Other names from NED --- Parameters of emission lines of galaxies Obs Note on observation number=1 *: Objects observed with the IPSC (6m telescope) **: Objects observed with the CCD (2.2m telescope) under poor photometric conditions --- Name Name of objects --- FHb H{beta}4861{AA} emission line observed flux 10-19W/m2 F[OII]/Hb [OII]3727{AA}/Hb emission line fluxes ratio --- F[OII] [OII]3727A emission line observed flux 10-19W/m2 F[OIII]/Hb [OIII]5007{AA}/Hb emission line fluxes ratio --- F[OIII] [OIII]5007A emission line observed flux 10-19W/m2 FHa/Hb Emission line fluxes ratio Ha/Hb --- FHa H{alpha} emission line observed flux 10-19W/m2 F[NII]/Ha [NII]6583{AA}/Ha emission line fluxes ratio --- F[SII]/Ha [SII](6716{AA}+6730{AA})/Ha emission line fluxes ratio --- W[OII] [OII]3727{AA} emission line equivalent width 0.1nm WHb H{beta} emission line equivalent width 0.1nm W[OIII] [OIII]5007{AA} emission line equivalent width 0.1nm Coordinates, redshifts and magnitudes of QSOs Name Name of objects --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec z Observed redshift --- Bmag Magnitude in B filter mag ELines Detected emission lines --- Galaxies without emission lines Name Name of objects --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec HRV Heliocentric radial velocity km/s Bmag Magnitude in B filter mag BMAG Absolute B-magnitude mag ALines Absorption lines --- Stars positions and spectral features Name Name of objects --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec n_Bmag *: Magnitudes are taken from the APM Maddox et al., Cat. <J/MNRAS/246/433> --- Bmag Magnitude in B filter mag Type Spectral type of a star --- Lines Spectral features --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1998 Dec 03 Andrew Ugryumov <and@relay.sao.ru> J_A+AS_135_511.xml uvby photometry of the magnetic CP stars HD 35298, 19 Lyrae, HD 192678, and HR 8216 J/A+AS/136/111 J/A+AS/136/111 uvby photometry of 4 CP stars uvby photometry of the magnetic CP stars HD 35298, 19 Lyrae, HD 192678, and HR 8216 S J Adelman R H Rice Astron. Astrophys. Suppl. Ser. 136 111 1999 1999A&AS..136..111A J/A+AS/103/1 : 63 And, HD 192913, HR 8240 & 108 Aqr (Adelman+ 1994) J/A+AS/106/333 : Alpha And, HD 184905, HR 8216 & HR 8434 (Adelman+ 1994) J/A+AS/111/41 : 56 Tauri, HD 111133, HD 126515 and HD 215441 (Adelman+ 1994) J/A+AS/114/253 : HD 11187, HD 14940, HD 15144, 20 Eri, HR 8933 (Adelman+ 1995) J/PASP/109/9 : HR 1643, Theta Aur, 49 Cam, and HR 3724 (Adelman 1997) J/A+AS/122/249 : HD32633, 25 Sex, HR 7224, and HD 200311 (Adelman, 1997) J/A+A/329/579 : uvby photometry of theta CrB (Fabregat+ 1998) J/A+AS/123/445 : uvby photometry of metallic + Hg-Mn stars (Adelman 1997) J/A+AS/125/65 : HD 37776, HR 2258, HR 6958 & 108 Aqu (Adelman, 1997) J/A+AS/125/497 : Theta Vir and 109 Vir uvby photometry (Adelman 1997) J/A+AS/128/245 : AR Aur, 3 Hya, 49 Cnc & BX Boo (Adelman 1997) J/A+A/333/952 : BVRI photometry of HR 1105 (Adelman 1998) J/A+AS/136/379 : 45 Leo, HR 4330, 49 Her and HR 6718 (Adelman+ 1999) Photometry, uvby Stars, peculiar stars: chemically peculiar stars: individual (HD 35298, 19 Lyr, HD 192678, HR 8216) Differential Stroemgren uvby observations from the Four College Automated Photoelectric Telescope are presented for the mCP stars HD 35298, 19 Lyr, HD 192678, and HR 8216. The period for HD 35298 of 1.85457 days is a revision of North's value while that for 19 Lyr of 7.0980 days is alias of that found by Winzer. HD 192678 is found to be a small amplitude photometric variable with the 6.4186 day period proposed by Leroy from polarization measurements. For HR 8216, observations taken between 1995 and 1998 confirm that the star has remained constant at least since 1990.
HD 35298 05 23 50.4 +02 04 56 HD 179527 19 Lyr 19 11 46.0 +31 17 00 HD 192678 20 13 36.3 +53 39 34 HR 8216 HD 204411 21 26 51.6 +48 50 07
Photometry of HD 35298 Photometry of 19 Lyr Photometry of HD 192678 New HR 8216 Photometry HJD Heliocentric Julian Date d umag1 variable-comparison (v-c) u magnitude mag umag2 check-comparison (ch-c) u magnitude mag vmag1 variable-comparison (v-c) v magnitude mag vmag2 check-comparison (ch-c) v magnitude mag bmag1 variable-comparison (v-c) b magnitude mag bmag2 check-comparison (ch-c) b magnitude mag ymag1 variable-comparison (v-c) y magnitude mag ymag2 check-comparison (ch-c) y magnitude mag Average photometry Table Number of table with detailed photometry --- Name Star name --- Per Period considered --- umag1 Variable-comparison (v-c) u magnitude mag e_umag1 rms uncertainty on umag1 mag umag2 Check-comparison (ch-c) u magnitude mag e_umag2 rms uncertainty on umag2 mag vmag1 Variable-comparison (v-c) v magnitude mag e_vmag1 rms uncertainty on vmag1 mag vmag2 Check-comparison (ch-c) v magnitude mag e_vmag2 rms uncertainty on vmag2 mag bmag1 Variable-comparison (v-c) b magnitude mag e_bmag1 rms uncertainty on bmag1 mag bmag2 Check-comparison (ch-c) b magnitude mag e_bmag2 rms uncertainty on bmag2 mag ymag1 Variable-comparison (v-c) y magnitude mag e_ymag1 rms uncertainty on ymag1 mag ymag2 Check-comparison (ch-c) y magnitude mag e_ymag2 rms uncertainty on ymag2 mag Patricia Bauer CDS 1999 Feb 19 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> J_A+AS_136_111.xml Photometric study of the late-type contact binary YY Eridani J/A+AS/136/139 J/A+AS/136/139 VB light curves of YY Eri Photometric study of the late-type contact binary YY Eridani Y Yang Q Liu Astron. Astrophys. Suppl. Ser. 136 139 1999 1999A&AS..136..139Y J/A+A/289/871 : YY Eri + AE Phe (Maceroni+, 1994) Binaries, eclipsing Photometry, UBV binaries: eclipsing stars: individual (YY Eri) The photoelectric observations in v and b bands for YY Eri are presented. These observations were obtained during four nights in November, 1984, with the 35-cm Cassegrain reflector of the Yunnan Observatory in China.
YY Eri BD-10 858 SAO 149449 04 12 08.8 -10 28 10 BD-11 831 04 13 28.1 -11 02 11
Individual observations for YY Eri in V colour Individual observations for YY Eri in B colour HJD Heliocentric Julian date d Dmag Magnitude difference (YY Eri - BD-11 831) mag Patricia Bauer CDS 1999 Feb 25 Yulan Yang <yang688@163.net> J_A+AS_136_139.xml Second San Juan photoelectric astrolabe catalogue J/A+AS/136/1 J/A+AS/136/1 CPASJ2 catalogue Second San Juan photoelectric astrolabe catalogue W T Manrique L Lu R Perdomo R C Podesta Z Wang E L Actis F Zeng Z Zeng E Alonso A M Pacheco G Bustos Astron. Astrophys. Suppl. Ser. 136 1 1999 1999A&AS..136....1M J/A+AS/118/1 : CPASJ1 catalogue (Lu+, 1996) J/other/PBeiO/24.71 : CPASJ1 position corrections (Lu+, 1994) I/143 : Fourth Fundamental Cat and Suppl (FK4, FK4S) (Fricke+ 1963) I/149 : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) - Extension (Fricke+ 1991) I/138 : The Southern Reference Star Catalogue (Smith+ 1989) I/147 : Carlsberg Meridian Catalog, Vol. 4 (CMC4, 1989) I/196 : Hipparcos Input Catalogue, Version 2 (Turon+ 1993) Magnitudes Positional data Spectral types astrometry catalogs reference systems According to the cooperation between Beijing, San Juan and La Plata Astronomical Observatories, the photoelectric astrolabe Mark II(PAII) of the Beijing Astronomical Observatory was moved and installed at the San Juan Observatory, Argentina in January, 1992 for observations of the catalogue of stars in the southern hemisphere. The first observing period was from Feb. 23, 1992 to Mar. 31, 1997. Using the data observed in San Juan with the instrument during this period, residuals for 11002 stars are reduced from about 405700 observations of stars over 1532 days. The mean precision of the residuals is +/-0.043". The Second Catalogue of Stars (CPASJ2) has been compiled from double transits at both the eastern and western passages. There are 5241 stars in this catalogue, including 1225 FK5/FK4Supp stars, 794 FK5Ext stars, 1084 SRS stars, 937 CAMC4 stars, 310 GC stars and 891 IMF stars. The mean precisions are +/-3.2ms and +/-0.057" in right ascension and declination, respectively. The magnitudes of stars are from 2.0 to 11.5. The declinations are from -3{deg} to -60{deg}. The mean epoch is 1994.9. Finally, systematic corrections of(CPASJ2-FK5) are given.
Second Catalogue of Stars with Photoelectric Astrolabe in San Juan CPASJ2 This catalogue reference number --- No Catalogues number number=1 No 1 to 467, FK5, Cat. <I/149> No 468 to 989, FK4Supp, Cat. <I/143> No 990 to 1647, FK5Ext, Cat. <I/175> No 1648 to 2034, SRS, Cat. <I/138> No 2035 to 2715, CAMC4, Cat. <I/147> No 2716 to 2908, GC, Cat. <I/133> No 2909 to 2980, Hipparcos Input Catalog, Cat. <I/196> --- Vmag Visual magnitude mag SpType Spectral type --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s pmRA Proper motion in RA (J2000.0) s/ha DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec DRA Position correction on right ascension ms pmDE Proper motion in DE (J2000.0) arcsec/ha e_DRA rms uncertainty on DRA ms DDE Position correction on declination 0.01arcsec e_DDE rms uncertainty on DDE 0.01arcsec Ne Eastern transit number of observations --- Nw Western transit number of observations --- Epoch Mean epoch of observation yr Patricia Bauer CDS 1998 Dec 10 podesta <podesta@iinfo.unsj.edu.ar> J_A+AS_136_1.xml CCD astrometry of Saturn's satellites in 1995 and 1997 J/A+AS/136/257 J/A+AS/136/257 Saturn's satellites in 1995/97 CCD astrometry of Saturn's satellites in 1995 and 1997 D Harper K Beurle I P Williams C D Murray D B Taylor A Fitzsimmons I M Cartwright Astron. Astrophys. Suppl. Ser. 136 257 1999 1999A&AS..136..257H J/A+AS/121/65 : 1990-1994 Saturn's satellites astrometry (Harper+ 1997) Planets Positional data planets and satellites: satellites of Saturn astrometry In this paper, we publish measurements of 1514 positions of the major satellites of Saturn made in 1995 and 1997 using CCD detectors attached to the 1-metre Jacobus Kapteyn Telescope on the island of La Palma. Analysis of the data as inter-satellite positions shows that the observations of Tethys, Dione, Rhea and Titan have root-mean-square residuals of 0.08 arc-seconds in 1995 and 0.10 arc-seconds in 1997.
Observations made in 1995 Observations made on 1997 October 21-22 Observations made on 1997 October 22-23 Observations made on 1997 October 23-24 OBS.Y Year of the observation number=1 U.T.C. time of the start of the exposure yr OBS.M Month of the observation number=1 U.T.C. time of the start of the exposure "month" OBS.D Day of the observation number=1 U.T.C. time of the start of the exposure d Exp Length of the exposure number=2 Add half of this value to the start date to obtain the mid-exposure time s Flags Boolean flags indicating presence (1) or absence (0) of each satellite in the image --- xiMimas Mimas {xi} column coordinate, if present pix etaMimas Mimas {eta} row coordinate, if present pix xiEnc Enceladus {xi} column coordinate, if present pix etaEnc Enceladus {eta} row coordinate, if present pix xiTethys Tethys {xi} column coordinate, if present pix etaTethys Tethys {eta} row coordinate, if present pix xiDione Dione {xi} column coordinate, if present pix etaDione Dione {eta} row coordinate, if present pix xiRhea Rhea {xi} column coordinate, if present pix etaRhea Rhea {eta} row coordinate, if present pix xiTitan Titan {xi} column coordinate, if present pix etaTitan Titan {eta} row coordinate, if present pix xiHyp Hyperion {xi} column coordinate, if present pix etaHyp Hyperion {eta} row coordinate, if present pix xiIap Iapetus {xi} column coordinate, if present pix etaIap Iapetus {eta} row coordinate, if present pix Patricia Bauer CDS 1999 Apr 06 David Harper <david@obliquity.u-net.com> J_A+AS_136_257.xml The photographic observations on the components of Sirius J/A+AS/136/293 J/A+AS/136/293 Sirius photographic observations The photographic observations on the components of Sirius D M D Jasinta B Hidayat Astron. Astrophys. Suppl. Ser. 136 293 1999 1999A&AS..136..293J Positional data Stars, double and multiple astrometry binaries: visual stars: individual (Sirius) A series of photographic observations on the components of Sirius was carried out in the years 1976-1986 at the Bosscha Observatory. We present the analysis and the results of the measurements.
Sirius 06 45 10.8 -16 41 58
Individual observational data on Sirius Plate Plate number --- Epoch Epoch of observation yr DRAcosDE Mean value of {DELTA}{alpha}cos{delta} arcsec e_DRAcosDE Mean error of DRAcosDE mas DDE Mean position of {DELTA}{delta} arcsec e_DDE Mean error of DDE mas PA Position angle deg e_PA Mean error of position angle 0.01deg Sep Measured separation arcsec e_Sep Mean error of measured separation mas Cont Contraction of emulsion --- e_Cont Mean error of contraction of emulsion 0.0001 SepCor Corrected separation arcsec e_SepCor Mean error of corrected separation mas q_PA Weight of position angle --- q_SepCor Weight of corrected separation --- Nimages Number of images --- Obs Observer --- Weighted means of observations on Sirius EpPA Mean epoch for position angle yr PA Mean value of position angle deg q_PA Weight of mean value of position angle --- EpSepCor Mean epoch for corrected separation yr SepCor Mean value of corrected separation arcsec q_SepCor Weight of mean value of SepCor --- Nplates Number of plates --- Patricia Bauer CDS 1999 Jan 14 D.M.D. Jasinta <JASINTA@sirius.as.itb.ac.id> J_A+AS_136_293.xml An astrometric catalogue for the area of Coma Berenices J/A+AS/136/307 J/A+AS/136/307 Coma Berenices astrometric catalogue An astrometric catalogue for the area of Coma Berenices C Abad B Vicente Astron. Astrophys. Suppl. Ser. 136 307 1999 1999A&AS..136..307A Clusters, open Magnitudes, photographic Positional data Proper motions astrometry catalogs methods: data analysis open clusters and associations: individual (Coma cluster) A catalogue of stellar positions and proper motions down to the 14th photographic magnitude in the area of the open cluster in Coma Berenices is compiled from data of 12 different sources. The accuracy of the proper motion data is comparable to that of the Hipparcos Catalogue (Cat. <I/239>).
Catalogue for the area of Coma Berenices Seq Running number of this catalog --- Pmag Estimated photographic magnitude mag SpType Spectral type --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s e_RAs Mean error of right ascension ms pmRA Proper motion in right ascension s/yr e_pmRA Error of proper motion in right ascension 10-5s/yr DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec e_DEs Mean error of declination 10mas Epoch Epoch of right ascension and declination yr pmDE Proper motion in declination arcsec/yr e_pmDE Mean error of proper motion in declination 0.1mas/yr Depoch Maximum epoch difference yr Ncat Number of contributing catalogs --- Patricia Bauer CDS 1999 Jan 29 Carlos Abad <abad@cida.ve> J_A+AS_136_307.xml New catalogue of Wolf-Rayet galaxies and high-excitation extra-galactic HII regions J/A+AS/136/35 J/A+AS/136/35 WR galaxies and HII regions catalog New catalogue of Wolf-Rayet galaxies and high-excitation extra-galactic HII regions D Schaerer T Contini M Pindao Astron. Astrophys. Suppl. Ser. 136 35 1999 1999A&AS..136...35S http://www.obs-mip.fr/omp/astro/people/schaerer : Daniel Schaerer's Homepage Galaxy catalogs H II regions Radial velocities galaxies: ISM galaxies: starburst galaxies: stellar content stars: Wolf-Rayet We present a new compilation of Wolf-Rayet (WR) galaxies and extra-galactic HII regions showing broad He II {lambda}4686 emission drawn from the literature. Relevant information on the presence of other broad emission lines (N III {lambda}4640, C IV {lambda}5808 and other) from WR stars of WN and WC subtypes, and other existing broad nebular lines is provided. In total we include 139 known WR galaxies. Among these, 57 objects show both broad He II {lambda}4686 and C IV {lambda}5808 features. In addition to the broad (stellar) He II {lambda}4686 emission, a nebular He II component is well established (suspected) in 44 (54) objects. We find 19 extra-galactic HII regions without WR detections showing nebular He II {lambda}4686 emission. The present sample can be used for a variety of studies on massive stars, interactions of massive stars with the ISM, stellar populations, starburst galaxies etc. The data is accessible electronically and will be updated periodically
List of WR galaxies (all WR populations outside Local Group) Name Object name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec MType Morphological type --- Bmag Apparent B magnitude mag HRV Heliocentric radial velocity km/s r_HeII Comma-separated list of references number=1 References of the first publication indicating the presence of broad He II {lambda}4686. (C91) stands for objects included in Conti (1991ApJ...377..115C) catalogue. The complete references are in refs.dat file --- HeII Existence of nebular He II {lambda}4686 number=2 no entry: information not available -: absent ?: possible/suspected !: present, but no data available UL: upper limit available Q: measurement available --- r_CIV Comma-separated list of references about broad CIV {lambda}5808 line number=3 Reference to the first detection of broad C IV {lambda}5808, exceptionally also other broad features, cf. NGC 1365. The complete references are in refs.dat file --- List of extragalactic regions with nebular Name Object name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec MType Morphological type --- Bmag Apparent B magnitude mag HRV Heliocentric radial velocity km/s r_HRV Comma-separated list of references (see refs.dat file) --- Com Comment --- List of suspected WR galaxies Name Object name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Bmag Apparement B magnitude mag HRV Heliocentric radial velocity km/s r_HRV Comma-separated list of references (see refs.dat file) --- References Ref Ref designation --- BibCode BibCode --- Aut Author names --- Com Comments --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1999 Feb 02 Thierry Contini <tcontini@eso.org> J_A+AS_136_35.xml Orbits of new spectroscopic components in 8 multiple systems J/A+AS/136/373 J/A+AS/136/373 Orbits of 8 multiples Orbits of new spectroscopic components in 8 multiple systems A A Tokovinin Astron. Astrophys. Suppl. Ser. 136 373 1999 1999A&AS..136..373T J/A+AS/124/75 : Multiple star catalogue (MSC) (Tokovinin 1997) J/PAZh/24/343 : New spectroscopic components (Tokovinin, 1998) Binaries, spectroscopic Radial velocities Stars, double and multiple binaries: spectroscopic binaries: visual New close sub-systems are discovered in 8 visual late-type double stars. Elements of spectroscopic orbits (4 double-lined and 4 single-lined) are given for the components of quadruple systems ADS 1134 and 11163, for the components of triple systems ADS 455, 497, 5436, 8236, 10044, and for the primary of the optical pair ADS 9444. Magnitudes, colors, spectral types, masses of individual components are estimated by combining all available data with Hipparcos parallaxes. Among these stellar systems we note a subdwarf triple ADS 497, an old system with subgiant components ADS 10044, and a visual triple ADS 11163 with additional very low mass (possibly substellar) spectroscopic companion in a 4.6 day orbit. The astrometric orbit of ADS 8236B with a semimajor axis of 30 mas and a period of 4.6 yr may be recoverable from Hipparcos data.
ADS 455 HD 2942 2583 00274+2744 HR 134 00 32 49.1 +28 16 49 ADS 497 HD 3266 2844 00307+2927 LTT 10205 00 36 02.4 +29 59 35 ADS 1134 HD 8610/24 6668 01200+3102 STT 30 01 25 34.3 +31 33 01 ADS 5436 HD 48766/67 32609 06399+5549 HR 2486/85 06 48 12.3 +55 42 15 ADS 8236 HD 100831 8236 11311+5642 STF 1553 11 36 35.7 +56 08 07 ADS 9444 HD 132049 9444 14520+2953 STF 1893 14 56 15.4 +29 28 28 ADS 10044 HD 148086 10044 16206+3716 STF 2044 16 24 10.4 +37 02 12 ADS 11163 BD +84 409 11163 18199+8434 HU 65 18 01 24.9 +84 35 49
Radial velocities and residuals Name Star name --- HJD Heliocentric Julian Date d RV Radial velocity km/s e_RV Formal error of radial velocity km/s O-C Residual velocity to the orbit solution km/s Rem Remarks, see Note number=1 COR: CORAVEL measurement ":": Rejected in orbit computation --- Patricia Bauer CDS 1999 Feb 08 Tokovinin Andrei <toko@cumulus.univ-lyon1.fr> J_A+AS_136_373.xml uvby Photometry of the magnetic CP stars 45 Leonis, HR 4330, 49 Herculis, and HR 6718 J/A+AS/136/379 J/A+AS/136/379 uvby photometry of 4 CP stars uvby Photometry of the magnetic CP stars 45 Leonis, HR 4330, 49 Herculis, and HR 6718 S J Adelman K E Rayle C -L M Pi Astron. Astrophys. Suppl. Ser. 136 379 1999 1999A&AS..136..379A J/A+AS/103/1 : 63 And, HD 192913, HR 8240 & 108 Aqr (Adelman+ 1994) J/A+AS/106/333 : Alpha And, HD 184905, HR 8216 & HR 8434 (Adelman+ 1994) J/A+AS/111/41 : 56 Tauri, HD 111133, HD 126515 and HD 215441 (Adelman+ 1994) J/A+AS/114/253 : HD 11187, HD 14940, HD 15144, 20 Eri, HR 8933 (Adelman+ 1995) J/PASP/109/9 : HR 1643, Theta Aur, 49 Cam, and HR 3724 (Adelman 1997) J/A+AS/122/249 : HD32633, 25 Sex, HR 7224, and HD 200311 (Adelman, 1997) J/A+A/329/579 : uvby photometry of theta CrB (Fabregat+ 1998) J/A+AS/123/445 : uvby photometry of metallic + Hg-Mn stars (Adelman 1997) J/A+AS/125/65 : HD 37776, HR 2258, HR 6958 & 108 Aqu (Adelman, 1997) J/A+AS/125/497 : Theta Vir and 109 Vir uvby photometry (Adelman 1997) J/A+AS/128/245 : AR Aur, 3 Hya, 49 Cnc & BX Boo (Adelman 1997) J/A+A/333/952 : BVRI photometry of HR 1105 Photometry, uvby Stars, peculiar stars: chemically peculiar stars: individual (45 Leo, HR 4330, 49 Her, HR 6718) Differential Stroemgren uvby photometric observations from the Four College Automated Photoelectric Telescope are presented for the magnetic CP stars 45 Leo, HR 4330, 49 Her, and HR 6718. We refined Winzer's periods for 45 Leo and HR 6718 to 1.443820 days and 0.51899days, respectively. For HR 4330 our period of 3.516 days is quite different from that of Winzer. That for 49 Her, 0.93663days, is an alias of Winzer's.
HD 90569 45 Leo 10 27 39.0 +09 45 45 HR 4330 HD 96707 11 09 39.8 +67 12 37 HD 152308 49 Her 16 52 04.9 +14 58 27 HR 6718 HD 164429 17 58 52.3 +45 28 34
Photometry of 45 Leo Photometry of HR 4330 Photometry of 49 Her Photometry of HR 6718 HJD Heliocentric Julian Date d umag1 variable-comparison (v-c) u magnitude mag umag2 check-comparison (ch-c) u magnitude mag bmag1 variable-comparison (v-c) b magnitude mag bmag2 check-comparison (ch-c) b magnitude mag vmag1 variable-comparison (v-c) v magnitude mag vmag2 check-comparison (ch-c) v magnitude mag ymag1 variable-comparison (v-c) y magnitude mag ymag2 check-comparison (ch-c) y magnitude mag Average photometry Table Table number with detailed photometry --- Name Star name --- Years Period of observation --- umag1 Variable-comparison (v-c) u magnitude mag e_umag1 rms uncertainty on umag1 mag umag2 Check-comparison (ch-c) u magnitude mag e_umag2 rms uncertainty on umag2 mag vmag1 Variable-comparison (v-c) v magnitude mag e_vmag1 rms uncertainty on vmag1 mag vmag2 Check-comparison (ch-c) v magnitude mag e_vmag2 rms uncertainty on vmag2 mag bmag1 Variable-comparison (v-c) b magnitude mag e_bmag1 rms uncertainty on bmag1 mag bmag2 Check-comparison (ch-c) b magnitude mag e_bmag2 rms uncertainty on bmag2 mag ymag1 Variable-comparison (v-c) y magnitude mag e_ymag1 rms uncertainty on ymag1 mag ymag2 Check-comparison (ch-c) y magnitude mag e_ymag2 rms uncertainty on ymag2 mag Patricia Bauer CDS 1999 Feb 19 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> J_A+AS_136_379.xml Atomic data from the Iron Project. XXXVII. Electron impact excitation collision strengths and rate coefficients for Fe VI J/A+AS/136/395 J/A+AS/136/395 IRON Project XXXVII. Fe VI collision strengths Atomic data from the Iron Project. XXXVII. Electron impact excitation collision strengths and rate coefficients for Fe VI G X Chen A K Pradhan Astron. Astrophys. Suppl. Ser. 136 395 1999 1999A&AS..136..395C Atomic physics electron collision rates fine structure transitions HII regions planetary nebulae: general stars: hot white dwarfs Collision strengths and Maxwellian-averaged rate coefficients have been calculated for 3,160 non-vanishing transitions among 80 fine structure levels, dominated by configurations 3d^3^, 3d^2^4s, and 3d^2^4p in Fe VI. Collision strengths are calculated using the R-matrix method with a 34-term close-coupling target expansion and for electron energies up to 10 Rydbergs. Detailed comparisons of rate coefficients are presented with the relativistic Breit-Pauli calculations using a 19-level expansion corresponding to the first 8 LS terms dominated by the ground configuration 3d^3^. For the low-lying transitions of practical interest there is excellent agreement, better than 10%, among three sets of rate coefficients calculated using 34 term and 8-term non-relativistic calculations and the 19-level Breit-Pauli calculation, indicating that (i) the relativistic effects are not too significant, and (ii) the numerical uncertainties associated with the resolution of the extensive resonances in the collision strengths are small. Rate coefficients are tabulated in a range of temperatures, 10^4^-10^6^K, where Fe VI is normally abundant in radiatively photoionized or collisionally ionized plasmas sources. The present rates for Fe VI are expected to find applications in UV spectral diagnostics of hot stellar sources and planetary nebulae.
Levels for table4 Index Level index --- 2J Twice total angular momentum --- E Experimental energy Ry Term configuration and electronic term --- Patricia Bauer CDS 1999 Jun 17 Guo-xin Chen <chen@astronomy.ohio-state.edu> UNKNOWN UNKNOWN * 02-Apr-1999: first version * 17-Jun-1999: table4 was updated (new version supplied by the author) * 18-Jul-1999: table4 newly updated (a newer version supplied by the author) J_A+AS_136_395.xml A search for spectroscopic binaries among Herbig Ae/Be stars J/A+AS/136/429 J/A+AS/136/429 Herbig Ae/Be stars candidates A search for spectroscopic binaries among Herbig Ae/Be stars P Corporon A -M Lagrange-Henri Astron. Astrophys. Suppl. Ser. 136 429 1999 1999A&AS..136..429C Binaries, spectroscopic Magnitudes Spectral types binaries: spectroscopic stars: early-type stars: pre-main sequence stars: statistics We have observed 42 Herbig Ae/Be stars candidates in both hemispheres using the high resolution spectrographs AURELIE and ELODIE at OHP, and CES at ESO. Table 1 present the journal of our spectroscopic observations.
Journal of the observation Name Star name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude from SIMBAD mag SpType Spectral type from SIMBAD --- JD Julian date of observation d Instr Instrument name --- lambda Central wavelength of the spectrum number=1 535.0 : ELODIE spectra cover the 390.0-680.0 nm domain nm ExpTime Exposure time s Corporon LAOG-UdM Patricia Bauer CDS 1998 Nov 18 Patrice Corporon <corporon@ASTRO.UMontreal.CA> J_A+AS_136_429.xml CCD observations of Nereid and a new orbital determination J/A+AS/136/445 J/A+AS/136/445 CCD observations of Nereid CCD observations of Nereid and a new orbital determination C Veiga R Vieira Martins C Le Guyader Astron. Astrophys. Suppl. Ser. 136 445 1999 1999A&AS..136..445V J/A+AS/120/107 : 1989-1994 CCD observations of Triton (Veiga+ 1996) J/A+AS/131/291 : 1995-1997 CCD positions of Triton (Veiga+ 1998) Planets Positional data astrometry planets and satellites: individual (Nereid) 229 CCD positions of Nereid taken between 1993 and 1998 are presented. Many of the observations were taken near the periapsis. Considering also the other published positions we have a good distribution of the observations on the eccentric orbit of the satellite. Using a numeric integration method we fitted all these observations in order to determine one state vector for the orbit. The observed minus calculated standard deviation for all observations is 0.23", and for our observations it is 0.16".
List of observed positions of the Neptunian satellite Obs.Y Mean observation date (year) yr Obs.M Mean observation date (month) --- Obs.D Mean observation date (day) d Name Name of the satellite --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec List of observed positions of the Neptunian satellite relative to Triton Obs.Y Mean Observation date (year) yr Obs.M Mean Observation date (month) --- Obs.D Mean Observation date (day) d Name Name of the satellite, referred to Triton --- DRAcodDE {Delta}{alpha}cos{delta} position (J2000.0) arcsec DDE {Delta}{delta} position (J2000.0) arcsec Patricia Bauer CDS 1999 Feb 02 Carlos Henrique Veiga <cave@obsn.on.br> J_A+AS_136_445.xml An abundance analysis of the single-lined spectroscopic binaries with barium stars-like orbital elements. II. The spectroscopic data. J/A+AS/136/453 J/A+AS/136/453 Equivalent widths of spectroscopic binaries An abundance analysis of the single-lined spectroscopic binaries with barium stars-like orbital elements. II. The spectroscopic data. L Zacs O Alksnis F A Musaev I F Bikmaev G A Galazutdinov Astron. Astrophys. Suppl. Ser. 136 453 1999 1999A&AS..136..453Z Binaries, spectroscopic Equivalent widths binaries: spectroscopic stars: abundances stars: chemically peculiar High-resolution spectroscopic observations are presented for 19 single-lined binaries (giants and dwarfs) with orbital elements and mass functions similar to those of barium stars, two radial velocity non-variable barium stars, and two standards. All binary systems contain an unseen low-mass component, presumably, a white dwarf. The equivalent widths and oscillator strengths are given for all measured spectral lines.
List of stars observed HD HD (Cat <III.135>) star number --- RAh Right Ascension J2000 (hours) number=1 data from SIMBAD h RAm Right Ascension J2000 (minutes) number=1 data from SIMBAD min RAs Right Ascension J2000 (seconds) number=1 data from SIMBAD s DE- Declination J2000 (sign) number=1 data from SIMBAD --- DEd Declination J2000 (degrees) number=1 data from SIMBAD deg DEm Declination J2000 (minutes) number=1 data from SIMBAD arcmin DEs Declination J2000 (seconds) number=1 data from SIMBAD arcsec Bmag B magnitude number=1 data from SIMBAD mag Vmag V magnitude number=1 data from SIMBAD mag SpType Spectral class number=1 data from SIMBAD --- Stellar equivalent widths for 9 stars observed Stellar equivalent widths for 12 stars observed HD HD (Cat. <III/135>) number number= this column is empty for table3.dat --- lambda Laboratory wavelength of line number= this column is empty for table3.dat 0.1nm Ion Ion designation number= this column is empty for table3.dat --- log(gf) Oscillator strength of line accepted this column is empty for table3.dat number= this column is empty for table3.dat --- EW Equivalent width number= this column is empty for table3.dat 0.1pm Patricia Bauer CDS 1999 Feb 25 Laimons Zacs <zacs@sisenis.latnet.lv> J_A+AS_136_453.xml Photometric monitoring of three BL Lac objects in 1993-1998 J/A+AS/136/455 J/A+AS/136/455 BVRI photometry of 3 BL Lac objects Photometric monitoring of three BL Lac objects in 1993-1998 J M Bai G Z Xie K H Li X Zhang W W Liu Astron. Astrophys. Suppl. Ser. 136 455 1999 1999A&AS..136..455B J/A+AS/98/393 : 1Jy BL Lac Objects: Observational Data (Stickel+ 1993) J/A+AS/106/361 : CCD Photometry of BL Lac objects (Xie+ 1994) J/AZh/71/717 : Polarimetric Observations of BL Lac (Gagen-Torn+ 1994) J/AJ/104/28 : JHKL photometry of BL Lac Objects (Bersanelli+ 1992) J/A+AS/116/403 : VRI photometry of stars in 12 BL Lac objects (Fiorucci+, 1996) J/A+AS/132/361 : Optical observations of eight BL Lacs (Raiteri+ 1998) J/A+AS/132/83 : BVRI photometry of 7 BL Lac objects (Bai+ 1998) BL Lac objects Photometry, UBVRI BL Lacertae objects: general BL Lacertae objects: individual (BL Lac, OJ 287, PKS 0735+178) galaxies: jets The results of optical photometric (BVRI) monitoring of three BL Lac objects over a time interval of about four years are presented. The sources are three classical radio-selected BL Lac objects, BL Lac, OJ 287 and PKS 0735+178. During our observation OJ 287 was in the stage of a large periodic outburst which consisted of at least two peaks. Almost all the observations obtained over consecutive nights detected intranight variations. In 1995 and 1996 BL Lac kept in faint states, with fewer and smaller rapid flares and fluctuations. On the contrary, in late 1997 BL Lac was at the stage of a large outburst, accompanied with much more large amplitude rapid flares and fluctuations. PKS 0735+178 was almost at its faint end from 1994 to early 1998. Over this time interval, the intraday variations and microvariations in PKS 0735+178 were rare and the amplitude was very small, except a rapid darkening of ~0.4mag on 24 January 1995. Previous work by Webb et al. (1988AJ.....95..374W), Wagner et al. (1996AJ....111.2187W) and Pian et al. (1997ApJ...486..784P) also showed the same behaviour of variability as BL Lac and PKS 0735+178 in BL Lac, S5 0716+714, PKS 2155-304, respectively. We propose that the motion of orientation of the relativistic jet in a BL Lac object be responsible for these variability behaviours.
BL Lac 22 02 43.4 +42 16 40 OJ 287 08 54 48.9 +20 06 31 PKS 0735+178 07 38 07.4 +17 42 19
Photometric data of three BL Lac objects Date Observation date "DD/MM/YY" JD Julian Date d mag Magnitude mag e_mag rms uncertainty on mag mag Band Filter used for the magnitude --- Object Name of the object observed --- Patricia Bauer CDS 1999 Feb 22 J.M. Bai <baijm@163.net> J_A+AS_136_455.xml Star formation in the Vela Molecular Clouds. III. Near infrared images and mm photometry of D-cloud IRAS sources. J/A+AS/136/471 J/A+AS/136/471 JHK photometry of D-cloud IRAS sources Star formation in the Vela Molecular Clouds. III. Near infrared images and mm photometry of D-cloud IRAS sources. F Massi T Giannini D Lorenzetti R Liseau A Moneti P Andreani Astron. Astrophys. Suppl. Ser. 136 471 1999 1999A&AS..136..471M Photometry, infrared Stars, pre-main sequence infrared: stars ISM: individual (Vela clouds) stars: formation stars: pre-main sequence Results of NIR (JHK) photometry for about 1300 stars in 12 fields around IRAS sources previously identified as Class I sources towards the Vela Molecular Ridge D-cloud. Only objects at least detected in the K band are listed. IRAS sources are indicated by the short designation adopted in the Paper (# IRS). Due to the presence of bad pixels or because of the closeness to the image edge, photometry could not be performed on a few objects and in such cases magnitudes and errors are not given at all. Note that as for IRS 13, coordinates are offsets (in arcsec) from source # 29.
JHK of about 1300 sources IRAS IRAS source (shortly designated as in Paper) --- ID Source designation --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Jmag J (1.24um) magnitude mag e_Jmag Photometric error on Jmag number=1 If unspecified, the magnitude is an upper limit mag Hmag H (1.63um) magnitude mag e_Hmag Photometric error on Hmag number=1 If unspecified, the magnitude is an upper limit mag Kmag K (2.19um) magnitude mag e_Kmag Photometric error on Kmag mag Notes Notes number=2 IN: integrated brightness of nebular emission BN: possible blob of nebular emission KS: possible saturation in K band JH: possible saturation in J and H bands AB: possible saturation in J, H and K bands --- oRA Offset in right ascension from IRS13 29 for IRS13 sources number=3 Unfortunately, we could not perform astrometry on field IRS13 since there are too few NIR sources with visible counterparts whose positions are listed in the GSC. Hence, we were forced to assign offsets from a reference objects. The position of the centre of the IRAS uncertainty ellipse, which, although probably near it, does not correspond to that of source 29. This is RA = 08:37:31.8 DE = -41:09:14 (1950). arcsec oDE Offset in declination from IRS13 29 for IRS13 sources number=3 Unfortunately, we could not perform astrometry on field IRS13 since there are too few NIR sources with visible counterparts whose positions are listed in the GSC. Hence, we were forced to assign offsets from a reference objects. The position of the centre of the IRAS uncertainty ellipse, which, although probably near it, does not correspond to that of source 29. This is RA = 08:37:31.8 DE = -41:09:14 (1950). arcsec Patricia Bauer CDS 1999 Apr 06 Fabrizio Massi <massi@coma.mporzio.astro.it> J_A+AS_136_471.xml Stellar kinematical data for the central region of spiral galaxies. II. J/A+AS/136/509 J/A+AS/136/509 Stellar kinematics in spiral galaxies. II. Stellar kinematical data for the central region of spiral galaxies. II. P Heraudeau F Simien G Maubon P Prugniel Astron. Astrophys. Suppl. Ser. 136 509 1999 1999A&AS..136..509H J/A+AS/133/317 : Stellar kinematics in spiral galaxies. I. (Heraudeau+ 1998) Galaxies, rotation Radial velocities Rotational velocities Velocity dispersion galaxies: general galaxies: kinematics and dynamics galaxies: spiral We present a second dataset of absorption spectroscopy on the inner region of spiral galaxies. We have determined the central velocity dispersion for 42 Sa-Sc objects and, for 32 of them, stellar rotation curves and velocity-dispersion profiles. Some of these profiles are limited to the bulge, some others do reach a region dominated by the luminosity of the disk. These data are intended to provide basic material for the study of the mass distribution and dynamical status in the central regions of spiral galaxies. Although no elaborate bulge-and-disk photometric decomposition is performed, we estimate the effects of limited resolution and contamination by disk light on the central velocity dispersion of the bulge. All the material presented in this paper, in particular the spectra, is available on-line.
Catalog elements and kinematical results Name Object identification --- Mtype Morphological type parameters Mtype through -Mb are catalog elements from the LEDA database (status: LEDA1998). parameters HRV through fbulge are determinations of the present work --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Btc Corrected integrated blue magnitude mag D25 Diameter at 25 B mag/arcsec**2 arcmin Eps Ellipticity --- PA Position angle of major axis PA (North --> East) as given in the range [0, 180[ by the LEDA database (status: LEDA1998). deg Mb Absolute blue magnitude Mb calculated from Btc and kinematical distance modulus, with H=75 km/s/Mpc mag HRV Heliocentric radial velocity km/s u_HRV Uncertainty flag on HRV --- e_HRV Mean error on HRV km/s sig0 Central velocity dispersion km/s u_sig0 Uncertainty flag on sig0 --- e_sig0 Mean error on sig0 km/s fbulge Resolution effect on bulge kinematics --- Log of the observations Name Object identification --- Date Date of observation "DD/MM/YY" Setup Spectrograph setup Setup=1 corresponds to a dispersion of 66{AA}/mm Setup=2 corresponds to a dispersion of 33{AA}/mm (not used in the present subsample; presence of this column is justified by the similarity of format with Paper I, 1998, Cat. <J/A+AS/133/317>). --- PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with the following convention on the subsequent radius r in the profiles (Table 3): - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg Nexp Number of exposures --- Texp Exposure time min Seeing Seeing FWHM arcsec u_Seeing Uncertainty flag on Seeing --- Profiles of velocity dispersion and rotation Name Object identification --- PA Position angle of slit PA (North --> East) is in the range [0, 360[, and with the following convention: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. deg r Radius (<0 and >0 on opposite semi-axes) arcsec Vrot Proj. mean stellar rotation velocity Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0. km/s e_Vrot Mean error on Vmag km/s sigma Projected velocity dispersion km/s e_sigma Mean error on sigma km/s Patricia Bauer CDS 1999 May 03 Francois Simien <fs@cumulus.univ-lyon1.fr> J_A+AS_136_509.xml Multi-period pulsation and amplitude variations behavior in delta Scuti variable DQ Cephei J/A+AS/136/515 J/A+AS/136/515 DQ Cephei amplitude variations Multi-period pulsation and amplitude variations behavior in delta Scuti variable DQ Cephei Z P Li M J Fang Astron. Astrophys. Suppl. Ser. 136 515 1999 1999A&AS..136..515L Magnitudes Stars, variable delta Scuti stars: individual (DQ Cep) stars: oscillations A period analysis of the data obtained in six nights of differential photoelectric photometry of the {delta} Scuti star DQ Cephei (about 42 hours) confirms the pulsation modes of f_1_=8.0480 cycle per day and f_2_=12.6826 cycle per day. The result adjusts well to the observations that cover a time span of 46 years. Comparing with the results obtained for different years, we discovered obvious amplitude variations of the two modes. These amplitude variations show phase differences of almost 180 degrees. The variation period probably is longer than 46 years.
DQ Cep HD 199908 20 57 48.4 +55 29 14 SAO 33038 HD 200017 20 58 27.1 +55 39 00
Photoelectric measurements of DQ Cephei relative to SAO 33038 (1997) JHD Heliocentric Julian date d Vmag V magnitude relative to SAO 33038 mag Patricia Bauer CDS 1998 Nov 03 Li Zhi ping <lizhi@class1.bao.ac.cn> J_A+AS_136_515.xml Central Mg_2_ indices for early-type galaxies. J/A+AS/136/519 J/A+AS/136/519 Mg2 indices for early-type galaxies Central Mg_2_ indices for early-type galaxies. V Golev P Prugniel F Simien M Longhetti Astron. Astrophys. Suppl. Ser. 136 519 1999 1999A&AS..136..519G J/A+AS/132/255 : A catalogue of Mg_2_ indices (Golev+ 1998) J/A+A/309/749 : Fundamental plane of early type galaxies (Prugniel+ 1996) http://www-obs.univ-lyon1.fr/hypercat/ : the HYPERCAT database Abundances, peculiar Galaxy catalogs galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: stellar content We present 210 new measurements of the central absorption line-strength Mg_2_ index for 87 early-type galaxies drawn from the Prugniel & Simien (1996, Cat. <J/A+A/309/749>) sample. 28 galaxies were not observed before. The results are compared to measurements published previously as available in HYPERCAT, and rescaled to the Lick system. The mean individual internal error on these measurements is 0.009mag+/-0.003mag and the mean external error is 0.012mag+/-0.002mag for this series of measurements. These data are also available from HYPERCAT.
Individual measurements Name Normalized galaxy identifier The Name has been adopted by descending the hierarchy: 1) NGC (Cat. <VII/118>) 2) IC (Cat. <VII/118>) 3) UGC (Cat. <VII/26>) 4) PGC (Cat. <VII/119>) Lyon-Meudon Extragalactic Database internal identifier, also acronimed PGC for numbers greater than 73097. The galaxy identifiers follow the rule already used in Prugniel & Simien, 1996, Cat. <J/A+A/309/749> and in Prugniel et al. 1998, Cat. <J/A+AS/127/117>. --- Obj Object type flag The type of the object (G=galaxy). Not usefull here, it is given only to follow the file format defined in <J/A+AS/132/255>, table1 --- RAh Right Ascension (1950) (hours) h RAm Right Ascension (1950) (minutes) min RAs Right Ascension (1950) (seconds) s DE- Declination (1950) (sign) --- DEd Declination (1950) (degrees) deg DEm Declination (1950) (minutes) arcmin DEs Declination (1950) (seconds) arcsec Mg2 Measured Mg2 index strength The Mg_2-index in magnitudes, corrected for velocity dispersion. mag e_Mg2 Uncertainty of Mg2 index strength mag Data Dataset acronym Dataset acronym which refers to the observational parameters in table3.dat --- n_Mg2c Measurement status flag The status flag of Mg_2_ index measurement which means as follows: 0= regular measurement; 1= discrepant measurement. --- Mg2c Corrected Mg2 index strength The aperture corrected and zero-pointed value of the Mg2 index. mag e_Mg2c Uncertainty on Mg2c mag Notes Description Descriptive notes. Not usefull here, kept only to follow the file format defined in Cat. <J/A+AS/132/255>, table1 --- Dataset parameters Data Dataset acronym --- Datc Correction method flag Flag for aperture correction of the dataset, which is always 0, i.e. no aperture correction. Kept for consistency with Cat. <J/A+AS/132/255>, table2 --- Xaper Aperture size in X direction The aperture sizes X x Y in arcsec. arcsec Yaper Aperture size in Y direction arcsec ExtError Estimated external error rms of the difference between the corrected measurements and the mean value for each galaxy. mag ZeroPoint Zero-point correction The dataset mean zero-point correction (corrected catalogue - dataset average), the r.m.s. error on it, and the corresponding rescaling factor of the internal error of the dataset. Iteratively, for each galaxy in the catalog, the error-weighted average of Mg_2_ is computed using the internal error. Then the mean is determined as well as the rms residual for each dataset after summing over all galaxies. The mean residual gives the zero-point for the considered dataset, and its rms is an estimate of the external error. The comparison between the external error and the mean internal error allows to rescale the latter. mag Scal Rescaling factor of the internal error mag Ndata Number of measurements in dataset The number of measurements reported in the dataset. Not always equal to the number of observed objects (there are datasets which include multiple measurements of one object). --- Ncomp Number of comparison measurements The number of measurements used for comparison with the homogeneous system. --- Hmgnf Homogenisation flag Always 1, i.e. these measurements are rescaled to the homogeneous system of Mg_2_ values defined in Hypercat. Kept for consistency with Cat. <J/A+AS/132/255>, table2 --- Mean corrected Mg_2_ Name Normalized galaxy identifier --- RAh Right ascension (1950) Sorted by increasing of R.A. h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec RV Flow-smoothed corrected velocity The flow-smoothed velocity used for aperture correction (defined as the velocity of the cosmologic flow associated with the galaxy). It is determined iteratively by averaging the velocity of galaxies found in the neighbourhood of given galaxy. At each step the size of the neighbouring region (in radius on the sky and in velocity interval) is computed from the distribution of the galaxies grouped at the previous step. The source of velocities is HYPERCAT (in turn updated from LEDA). The flow-smoothed velocity is then corrected for the deviations from the linear flow assuming the three-component velocity field model (Great Attractor, Virgocentric infall and Local Group Anomaly) described in Faber & Burstein (1988, in: Motions of galaxies in the neighbourhood of the local group, p.115) and Burstein et al. (1989, in Large-scale motions in the nearby universe, p. 179). km/s Mg2 Homogeneous Mg2 index strength Mean homogeneous value of the Mg2 index. mag e_Mg2 Uncertainty of Mg2 index strength mag n_Mg2 Number of individual measurements --- Patricia Bauer CDS 1999 May 10 Valeri Golev <valgol@phys.uni-sofia.bg> J_A+AS_136_519.xml CCD astrometry and instrumental DeltaV photometry of visual double stars. V. Differential measurements of pairs with angular separations 1" to 4" J/A+AS/136/525 J/A+AS/136/525 DeltaV photometry of visual double stars CCD astrometry and instrumental DeltaV photometry of visual double stars. V. Differential measurements of pairs with angular separations 1" to 4" D Sinachopoulos A Dapergolas E van Dessel E Kontizas Astron. Astrophys. Suppl. Ser. 136 525 1999 1999A&AS..136..525S J/A+AS/124/353 : CCD UBV photometry of close visual doubles (Nakos+ 1997) Sinachopoulos, Paper I. 1988A&AS...76..189S Sinachopoulos & Seggwiss, Paper II. 1990A&AS...83..245S Nakos et al., Paper IV. 1995A&AS..112..453N Stars, double and multiple astrometry binaries: visual We present angular separations, position angles and {Delta}V instrumental magnitude differences of 83 visual double stars with angular separations around two arcseconds. Our observations were made by means of a CCD detector attached to the Kryonerion 1.2m telescope. 12 of them are common proper motion stars and their components should therefore be stars of common origin.
CCD astrometry and {Delta}V photometry RAh Right ascension of the primary (J2000) h RAm Right ascension of the primary (J2000) min DE- Declination sign (2000) --- DEd Declination of the primary (J2000) deg DEm Declination of the primary (J2000) arcmin BD BD (Cat. <I/122>) number --- DVmag V differential magnitude mag e_DVmag rms uncertainty on DVmag mag rho Separation angle arcsec e_rho rms uncertainty on rho arcsec theta Position angle deg e_theta rms uncertainty on theta deg Epoch Epoch of observation yr table3.tex LaTeX version of table 3 Patricia Bauer CDS 1999 Mar 02 Anastasios Dapergolas <adaperg@titan.astro.noa.gr> J_A+AS_136_525.xml Observations of radio stars at the Valinhos CCD Meridian Circle J/A+AS/136/531 J/A+AS/136/531 Valinhos CCD Meridian Circle radio stars Observations of radio stars at the Valinhos CCD Meridian Circle P A A Lopes A H Andrei S Puliaev J L Penna R Teixeira P Benevides-Soares M Assafin J F Le Campion Y Requieme Astron. Astrophys. Suppl. Ser. 136 531 1999 1999A&AS..136..531L II/199 : Radio continuum emission form stars (Wendker, 1995) I/246 : The ACT Reference Catalog (Urban+ 1997) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Magnitudes Stars, radio astrometry radio continuum: stars reference systems The astrometry of 16 radio stars taken from the list of Wendker (1995, Cat. <II/199>) is presented. The observations were carried out between 1996.3 and 1998.8 at the Valinhos CCD Meridian Circle. The results are given on the Hipparcos/Tycho reference frame. The data obtained relatively to the ACT catalogue is presented here. The ACT reference stars measured on 16 sky strips are listed on the table named tableref. The Table 1 of this paper, is presented, giving the radio star position on each field.
Astrometry of 16 radio stars Name Radio star name --- TYC Tycho (ACT) identification --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag Visual magnitude mag o_Vmag Number of observations --- e_RAs Right ascension error (*cos{delta}) arcsec e_DEs Declination error arcsec JD Julian Date d ACT Reference stars positions SkyStrip Sky strip --- TYC Tycho (ACT) identification --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag Visual magnitude mag o_Vmag Number of observations --- e_RAs Right ascension error arcsec e_DEs Declination error arcsec JD Julian Date d Patricia Bauer CDS 1999 Jan 14 Paulo Afranio Augusto Lopes <afranio@obsn.on.br> J_A+AS_136_531.xml Pulsars identified from the NRAO VLA Sky Survey J/A+AS/136/571 J/A+AS/136/571 Pulsars identified from the NRAO VLA Sky Survey Pulsars identified from the NRAO VLA Sky Survey J L Han W W Tian Astron. Astrophys. Suppl. Ser. 136 571 1999 1999A&AS..136..571H VII/156 : Catalog of 558 Pulsars (Taylor+ 1993) Polarization Pulsars Radio sources polarization pulsars: general surveys Table1 gives the NVSS radio sources around the positions of all known pulsars. This table was generated by searching NVSS catalog, and each row gives the closest source around one pulsar. However, not all of them are pulsars, as we discussed in our paper. If there is "?" in the Notes, we had more considerations to identify the source as a pulsar. If there is nothing or just "*" in Notes, the source is believed to be the pulsar. Table 2 lists 14 strong pulsars not detected by the NVSS, or more exactly saying, not listed in the NVSS catalog. By the courtesy of Jim Condon, we found some of these pulsars are confused by nearby strong radio sources, and most of them were really scintillating during the NVSS.
NVSS sources around pulsar positions PSRJ Pulsar J-name --- PSRB Pulsar B-name --- RAh Right ascension (J2000) of pulsars h RAm Right ascension (J2000) of pulsars min RAs Right ascension (J2000) of pulsars s e_RAs uncertainty of pulsar position in RA s DE- Declination sign --- DEd Declination (J2000) of pulsars deg DEm Declination (J2000) of pulsars arcmin DEs Declination (J2000) of pulsars arcsec e_DEs Uncertainty of pulsar position in Dec arcsec MJD Modified Julian Date for pulsar position (JD-2400000.5) d S1.4GHz Pulsar flux density from pulsar catalog mJy RA2h Right ascension (J2000) of NVSS sources h RA2m Right ascension (J2000) of NVSS sources min RA2s Right ascension (J2000) of NVSS sources s e_RA2s uncertainty of source position in RA s DE2- Declination sign --- DE2d Declination (J2000) of NVSS sources deg DE2m Declination (J2000) of NVSS sources arcmin DE2s Declination (J2000) of NVSS sources arcsec e_DE2s Uncertainty of source position in Dec arcsec u_Delt Uncertainty flag on Delt --- Delt Angular distance between pulsar and source arcsec S1.4GHzR Flux density of the NVSS sources mJy e_S1.4GHzR Uncertainty of the flux density mJy L1.4GHzR Polarized Flux density of NVSS sources mJy e_L1.4GHzR uncertainty of the polarized flux density mJy L/S Polarization percentage % e_L/S Uncertainty of the polarization percentage --- PA Polarization angle of NVSS source deg e_PA Uncertainty of polarization angle deg Notes Short marks for Notes number=1 ?: more considerations in text of paper SNR: confused with supernova remnant no: confused with a strong sources nearby glbc: confused by host globular cluster *: new identifications not presented by Kaplan et al. (1998ApJS..119...75K) mode: PSR B1237+25 is in abnormal mode as comparing the PA with Fig.7 of Bartel et al. (1982ApJ...258..776B) --- Pulsars > 5 mJy but not detected by the NVSS PSRB Pulsar B-name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec S1.4GHz Flux density at 1.4 GHz from pulsar catalog mJy Type Conf.: confused; scin.; scintillated --- Patricia Bauer CDS 1999 Mar 08 Han JinLin <jhan@bac.pku.edu.cn> J_A+AS_136_571.xml A ROSAT PSPC X-Ray Survey of the Small Magellanic Cloud J/A+AS/136/81 J/A+AS/136/81 A ROSAT PSPC X-Ray Survey of the SMC A ROSAT PSPC X-Ray Survey of the Small Magellanic Cloud P Kahabka W Pietsch M D Filipovic F Haberl Astron. Astrophys. Suppl. Ser. 136 81 1999 1999A&AS..136...81K IX/11 : ROSAT Source Catalog (Voges+ 1994) Magellanic Clouds Surveys X-ray catalogs Magellanic Clouds supernova remnants X-rays: galaxies X-rays: stars We present the results of a systematic search for point-like and moderately extended soft (0.1-2.4keV) X-ray sources in a raster of nine pointings covering a field of 8.95deg^2^ and performed with the ROSAT PSPC between October 1991 and October 1993 in the direction of the Small Magellanic Cloud (SMC). We detect 248 objects which we include in the first version of our SMC catalogue of soft X-ray sources. We set up seven source classes defined by selections in the count rate, hardness ratio and source extent. We find five high luminosity super-soft sources (1E 0035.4-7230, 1E 0056.8-7146, RX J0048.4-7332, RX J0058.6-7146 and RX J0103-7254), one low-luminosity super-soft source RX J0059.6-7138 correlating with the planetary nebula L357, 51 candidate hard X-ray binaries including eight bright hard X-ray binary candidates, 19 supernova remnants (SNRs), 19 candidate foreground stars and 53 candidate background active galactic nuclei (and quasars). We give a likely classification for ~60% of the catalogued sources. The total count rate of the detected point-like and moderately extended sources in our catalogue is 6.9+/-0.3s^-1, comparable to the background subtracted total rate from the integrated field of ~6.1+/-0.1s^-1.
List of all 248 ROSAT sources found in the SMC Catalog Source catalog sequential number --- RX Source ROSAT name (Cat. <IX/11>) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Pe 90% confidence positional uncertainty arcsec Crate total count rate ct/ks e_Crate 1-sigma error of total count rate ct/ks HR1 soft hardness ratio HR1 --- e_HR1 1-sigma error of soft hardness ratio HR1 --- HR2 hard hardness ratio HR2 --- e_HR2 1-sigma error of hard hardness ratio HR2 --- EXT source extent arcsec LH likelihood ratio of existence --- Offax off-axis angle of source arcmin WW Source number of Einstein identification Wang & Wu, 1992ApJS...78..391W --- DistEinst Distance to Einstein source arcsec SpType Spectral type of Simbad star --- Mag Magnitude of Simbad identified star --- DistSim Distance to Simbad star arcsec Class Source classification number=1 A: background AGN or quasar B: hard X-ray binary Bl: luminous hard X-ray binary Bw: weak hard X-ray binary D: (possible) artifact F: foreground star R: supernova remnant or extended structure S: super-soft source Sl: luminous super-soft source Sw: weak super-soft source --- Class1 Refined source classification number=2 AB: class A or B (see Note 1) H: HII region --- Note Note on source classification --- Patricia Bauer CDS 1998 Dec 18 Peter Kahabka <ptk@astro.uva.nl> J_A+AS_136_81.xml On the nature of the Herbig Be star V380 Orionis J/A+AS/136/95 J/A+AS/136/95 V380 Ori emission line spectrum On the nature of the Herbig Be star V380 Orionis C Rossi L Errico M Friedjung F Giovannelli G Muratorio R Viotti A Vittone Astron. Astrophys. Suppl. Ser. 136 95 1999 1999A&AS..136...95R Equivalent widths Spectroscopy Stars, Be infrared: stars stars: emission-line, Be stars: individual (V380 Ori) stars: pre-main sequence ultraviolet: stars Table 3 presents the emission line spectrum of V380 Ori in the optical region observed at OHP in January 1995 with a mean resolution of 10000. For the line blends the wavelength and flux (not reddening corrected) of each contributor are given. For the P-Cygni profiles the equivalent widths of the absorption component are also reported. We estimate an error of less than 10% for the strongest lines, 10% to 40% for the weakest lines.
V380 Ori 05 36 25.3 -06 42 57
*The emission line spectrum of V380 Ori in January 1995 (OHP/AURELIE) LineID Identifier for successive lines number=1 When successive lines, they are preceded with the same identifier in the first column (from a to bh). --- n_LineID [1/6] Rank of the line number=2 For a set of lines, same n_LambdaObs, rank of the line. --- LambdaObs Observed heliocentric wavelength 0.1nm Flux Integrated emission line flux 10-13mW/m2/nm EW Absorption line equivalent width (Negative values) 0.1nm LambdaLab Laboratory wavelength 0.1nm Ion Ion of the contributor --- n_Ion Moore's multiplet number or Kurucz table (k) --- HRV Heliocentric radial velocity km/s Rem Remarks number=3 p: principal component b: blue shifted component pcy: P Cygni absorption component ca: narrow central/shell absorption is: interstellar absorption line contr: minor contributor to the line id?: uncertain identification --- table3.tex LaTeX version of table3 table3.ps PostScript version of table3 Patricia Bauer CDS 1999 Jan 11 Corinne Rossi <ROSSIC@axrma.uniroma1.it> J_A+AS_136_95.xml Near-infrared observations of galaxies in Pisces-Perseus: I. H-band surface photometry of 174 spirals J/A+AS/137/101 J/A+AS/137/101 H-band photometry in Pisces-Perseus spirals Near-infrared observations of galaxies in Pisces-Perseus: I. H-band surface photometry of 174 spirals G Moriondo C Baffa S Casertano G Chincarini G Gavazzi C Giovanardi L K Hunt D Pierini M Sperandio G Trinchieri Astron. Astrophys. Suppl. Ser. 137 101 1999 1999A&AS..137..101M Galaxies, photometry Morphology Photometry, infrared galaxies: fundamental parameters galaxies: spiral infrared: galaxies The paper presents results of an H-band imaging survey of spiral galaxies in the Perseus-Pisces supercluster area. The derived global photometric parameters of the sample galaxies (magnitudes, diameters, etc.) are collected in Table 3.
NIR global photometric parameters of the sample galaxies UGC UGC (U) or CGCG (C) number --- Figure Figure number, in fig4 subdirectory --- Name Other names --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec RH Revised Hubble type --- BTmag Blue total magnitude mag ADiam Major semiaxis (optical) arcmin BDiam Minor semiaxis (optical) arcmin HRV Heliocentric systemic velocity km/s HTmag H-band total magnitude mag H21.5 H-band isophotal magnitude mag u_H21.5 Extrapolation flag --- D21.5 H-band isophotal diameter arcmin u_D21.5 Uncertainty flag on D21.5 --- DHeff H-band effective diameter arcmin C31 Light concentration index --- Ell Outer ellipticity --- u_Ell Uncertainty flag --- PA Position angle deg u_PA Uncertainty flag number=1 When u_PA = X, the Position Angle is not determined (PA=999) --- Tel Telescope number=2 T: TIRGO telescope (Zermatt, Ch). Observations in 1992, 1993, 1994 and 1997. N: NOT telescope (La Palma, Canary Islands). Observations in 1995. V: VATT telescope (Mt Graham, Az). Observations in 1996. --- FWHM Seeing arcsec Comm Notes from catalogues --- C. Giovanardi Arcetri Patricia Bauer CDS 1999 Mar 26 Carlo Giovanardi <giova@arcetri.astro.it> J_A+AS_137_101.xml Five-colour photometry of OB-stars in the Southern Hemisphere. J/A+AS/137/113 J/A+AS/137/113 Walraven photometry of OB stars Five-colour photometry of OB-stars in the Southern Hemisphere. C J van Houten T Walraven J H Walraven Astron. Astrophys. Suppl. Ser. 137 113 1999 1999A&AS..137..113V Photometry, VBLUW Stars, early-type Stars, OB stars: colors stars: early-type Observations of OB-stars, made in 1959 and 1960 at the Leiden Southern Station near Hartebeespoortdam, South Africa, with the VBLUW photometer attached to th e 90 cm light-collector, are given in this paper. They are compared with photome try obtained by Graham (1968BANS....2..397G), Walraven & Walraven (1977BAN....15...67W), Lub & Pel (1977A&A....54..137L) and van Genderen et al. (1984A&AS...58..537V). Formulae for the transformation of the present observations to those of Walraven & Walraven (1977BAN....15...67W) and Lub & Pel (1977A&A....54..137L) are given. For a description of the VBLUW photometric system, see e.g. <GCPD/11>
Walraven VBLUW photometry (1959, 1960) HD/DM HD (Cat. <III/135>) number --- Nobs Number of observation used --- ObsYear Year were data was taken (10: 1959, 01: 1960, 11: 1959 and 1960) --- Vw Walraven V (log of intensity) --- (V-B)w Walraven V-B (log of intensity) --- (B-U)w Walraven B-U (log of intensity) --- (U-W)w Walraven U-W (log of intensity) --- (B-L)w Walraven B-L (log of intensity) --- Vmag Johnson V magnitude mag (B-V) Johnson B-V colour index mag table4.tex LaTeX version of table 4 Patricia Bauer CDS 1999 May 26 Jet Katgert <aanda@strw.leidenuniv.nl> J_A+AS_137_113.xml Recombination coefficients for the 5g-4f transitions of O III at nebular temperatures and densities J/A+AS/137/157 J/A+AS/137/157 O III recombination coefficients Recombination coefficients for the 5g-4f transitions of O III at nebular temperatures and densities R Kisielius P J Storey Astron. Astrophys. Suppl. Ser. 137 157 1999 1999A&AS..137..157K Atomic physics Planetary nebulae atomic data HII regions line: formation planetary nebulae: general We calculate effective recombination coefficients for the formation of the 5g-4f lines of O III in the intermediate coupling scheme. Photoionization data for the 5g levels calculated using the R-matrix method are used to derive their recombination coefficients. Cascading from higher states is included, allowing for the effects of finite electron density in a hydrogenic approximation. We explicitly include the distribution of population between the two ground levels of O^3+^ in the calculation of the line intensities. The results are presented as a simple programmable formula allowing the calculation of recombination line intensities for electron temperatures, T_e_ in the range 5000-20000K and electron densities, N_e_ in the range 10^2^-10^6^cm^-3^.
Indices n_1_ and energy levels of the 4f and 5g states in O^2+^ ions n1 Level index --- Term Term of parent level --- J0 J of parent level --- nl outer electron in spectroscopic notation --- S 2S+1 of level --- L L of level --- J J of level --- LK Experimental level assignment --- Jb J of level --- Exp Experimental level energy number=1 Experimental energy data are from Pettersson (Pettersson, Physica Scripta, 1982, 26, 296) while theoretical values are from SUPERSTRUCTURE (SS) and an R-matrix (RM) calculation. We also give our theoretical (SS) and previous experimental (Moore, 1970, "Atomic Energy Levels", NBS) level assignments. cm-1 SS Theoretical level energy from SUPERSTRUCTURE calculation cm-1 RM Theoretical level energy from R-matrix calculation cm-1 Wavelengths in air, electric dipole transition probabilities A(n_1_,n_2_) and branching ratios b(n_1_,n_2_) for the 5g-4f transitions in O^2+^ ions n1 Index of upper level number=1 The indices n1 and n2 correspond to the energy level indices in table 1. --- n2 Index of lower level number=1 The indices n1 and n2 correspond to the energy level indices in table 1. --- Lambda Wavelengths (air) 0.1nm A(n1,n2) Dipole transition probability between upper and lower levels s-1 b(n1,n2) Transition branching ratio --- Fitting coefficients for the direct recombination coefficients a_dir_ to the 5g levels of O^2+^ n1 Index of upper level --- a1 Fitting coefficient a_1_ --- b1 Fitting coefficient b_1_ --- c1 Fitting coefficient c_1_ --- d1 Fitting coefficient d_1_ --- a2 Fitting coefficient a_2_ --- b2 Fitting coefficient b_2_ --- c2 Fitting coefficient c_2_ --- d2 Fitting coefficient d_2_ --- Fractions of the cascade contributions from each series to the recombination coefficients of the 5g levels of O^2+^ n1 Index of upper level number=1 Indices n1 correspond to the energy level indices from table 1. --- g1c Fraction of cascade contribution from the first series --- g2c Fraction of cascade contribution from the second series --- Calculated and fitted effective recombination coefficients for the 5g levels of O^2+^ at the electron temperatures T=10000K and T=20000K and the electron density N=10^3^cm^-3^. n1 Index of upper level number=1 Indices n1 correspond to the energy level indices from table 1. --- acal1 T=10000K calculated recombination coefficient 10-12cm3/s afit1 T=10000K fitted recombination coefficient 10-12cm3/s acal2 T=20000K calculated recombination coefficient 10-12cm3/s afit2 T=20000K fitted recombination coefficient 10-12cm3/s Patricia Bauer CDS 1999 Apr 27 Romas Kisielius <rk@star.ucl.ac.uk> J_A+AS_137_157.xml Atomic data from the IRON Project. XXXVIII. Electron impact excitation of the fine-structure transitions in the n=3 complex of Fe XV J/A+AS/137/165 J/A+AS/137/165 IRON Project XXXVIII. Fe XV Atomic data from the IRON Project. XXXVIII. Electron impact excitation of the fine-structure transitions in the n=3 complex of Fe XV W Eissner M E Galavis C Mendoza C Zeippen Astron. Astrophys. Suppl. Ser. 137 165 1999 1999A&AS..137..165E J/A+AS/103/273 : IRON Project II. IR collision strengths of C-like ions J/A+A/283/319 : IRON Project III. B-like ions J/A+AS/108/1 : IRON Project V. Collision strengths of O-like ions J/A+A/293/953 : IRON Project VI. Fe II collision strengths J/A+A/293/967 : IRON Project VII. Fe II radiative transitions J/A+AS/109/193 : IRON Project VIII. Electron excitation of Ti-like ions J/A+AS/119/509 : IRON Project XVII. Radiative transition in Fe III J/A+AS/119/523 : IRON Project XVIII. Electron impact for Fe III J/A+AS/120/361 : IRON Project XIX. Fe II radiative transitions J/A+AS/123/159 : IRON Project XXII. C and O radiative rates J/A+AS/123/575 : IRON Project XXIII. Fe XXII excitation rate coefficients J/A+AS/126/373 : IRON Project XXVII. Fe IV collision strengths J/A+AS/131/499 : IRON Project XXIX. Boron isoelectronic sequence J/A+AS/131/153 : IRON Project XXXI. Fe XII electron excitation J/A+AS/135/347 : IRON Project XXXV. Fe XXIV & Fe XXV oscillator strengths J/A+AS/136/395 : IRON Project XXXVII. Fe VI collision strengths 1993A&A...279..298H : IRON Project I. Goal and methods 1994A&AS..107...29S : IRON Project IV. Electron excitation of F-like ions 1995A&AS..110..209P : IRON Project IX. Electron excitation of Cl-like ion 1995A&AS..111..347G : IRON Project X. Si- & S-like ions IR collision strengths 1996A&AS..115..151S : IRON Project XI. Ar VI, K VII and Ca VIII fine-structure 1995A&AS..114..367B : IRON Project XII. V-like ions electron excitation 1996A&AS..115..551B : IRON Project XIII. Ni II & Fe II electron excitation 1996A&A...309..677S : IRON Project XIV. Fe XIV fine-structure transition 1996A&AS..118..157K : IRON Project XV. Electron excitation of He II & Fe XXVI 1996A&AS..119..105B : IRON Project XVI. Fe V oscillator strengths 1997A&AS..122..167B : IRON Project XX. Fe I oscillator strengths 1997A&AS..122..177P : IRON Project XXI. Fe I fine-structure transition 1997A&AS..126..105B : IRON Project XXIV. Fe XXIV electron excitation 1998A&AS..127..545B : IRON Project XXV. Fe XII electron excitation 1997A&AS..126..365B : IRON Project XXVI. Fe IV oscillator strengths 1998A&AS..129..161B : IRON Project XXVIII. F-like ions fine-structure trans. 1999A&AS..134..369S : IRON Project XXX. P III, S IV & Cl V collision data 1998A&AS..133..245G : IRON Project XXXII. Ar III effective collision strength 1999A&AS..135..159M : IRON Project XXXIII. Carbon radiative rates 1999A&AS..136..385E : IRON Project XXXIV. Fe XVI electron impact excitation 1999A&AS..137..175C : IRON Project XXXVI. Fe XXIII electron excitation Atomic physics atomic data Sun: corona As part of a systematic study of the collisional properties of Fe ions carried out by the IRON Project, electron excitation rates (effective collision strengths) are computed for all the fine-structure transitions within the n=3 complex of Fe XV in the electron temperature range 10^5^<=T/K<=10^7^. Configuration-interaction target wavefunctions are generated with the atomic structure code superstructure, and collision strengths are computed in the close-coupling approximation with a Breit-Pauli R-matrix package. Special care is taken to resolve the resonance structure and to ensure the convergence of the partial wave expansion, specially for dipole allowed transitions. By comparing with previously calculated collision strengths in the distorted wave approximation, a 20% accuracy rating is assigned to transitions with effective collision strengths {Upsilon}(T)>10^-2^.
Effective collision strength for the electron impact excitation of Fe XV. i Initial level --- j Final level --- gamma1 Effective collision strength for log(T)=5.0K --- gamma2 Effective collision strength for log(T)=5.2K --- gamma3 Effective collision strength for log(T)=5.4K --- gamma4 Effective collision strength for log(T)=5.6K --- gamma5 Effective collision strength for log(T)=5.8K --- gamma6 Effective collision strength for log(T)=6.0K --- gamma7 Effective collision strength for log(T)=6.2K --- gamma8 Effective collision strength for log(T)=6.4K --- gamma9 Effective collision strength for log(T)=6.6K --- gamma10 Effective collision strength for log(T)=6.8K --- gamma11 Effective collision strength for log(T)=7.0K --- table5.tex LaTeX version of table5 Patricia Bauer CDS 1999 Apr 20 Claude Zeippen <Claude.Zeippen@obspm.fr> J_A+AS_137_165.xml Elemental abundance studies of CP stars. II. The silicon stars HD 133029 and HD 192913 J/A+AS/137/227 J/A+AS/137/227 HD 133029 & HD 192913 elemental abundances Elemental abundance studies of CP stars. II. The silicon stars HD 133029 and HD 192913 Z Lopez-Garica S J Adelman Astron. Astrophys. Suppl. Ser. 137 227 1999 1999A&AS..137..227L J/A+AS/107/353 : Paper I. HD 43819, HD 147550 (Lopez-Garcia+, 1994) Abundances, peculiar Equivalent widths Stars, peculiar stars: abundances stars: chemically peculiar stars: individual (HD 133029, HD 192913) Fine analyses of the silicon stars HD 133029 and HD 192913 are presented using ATLAS9 model atmospheres whose predictions fit the optical region spectrophotometry and H{gamma} profiles and have the same bulk metallicity as the deduced abundances. Both are very He poor stars. The light elements are mostly solar except for silicon, and all the heavier elements, except nickel in HD 133029 which is solar, are greatly overabundant. The iron peak elements are typically 10 times overabundant. SrYZr are of order of 100 times solar. The rare earths are 1000 or more times overabundant.
HD 133029 15 00 38.7 +47 16 39 HD 192913 20 16 27.2 +27 46 34
Elemental abundances El Element --- No Multiplet Number --- Lambda Wavelength 0.1nm log(gf) Oscillator strength --- r_log(gf) Reference to oscillator strength number=1 Sources of gf-values: BG = Biemont et al. (1981ApJ...248..867B) BK = Biemont et al. (1982A&A...107..166B) DW = Dworetsky (1980A&A....84..350D) GB = Grevesse et al. (1981, Upper Main Sequence CP Stars, 23rd. Liege Astrophys. Coll., 211) HL = Hannaford et al. (1982ApJ...261..736H) KX = Kurucz (1992RMxAA..23...45K) LA = Lanz & Artru (1985PhyS...32..115L) MC = Magazzu & Cowley (1986ApJ...308..254M) MF = Martin, Fuhr & Wiese (1988, Cat. <VI/72>) for Sc through Mn; Fuhr, Martin & Wiese (1988, Cat. <VI/72>) for Fe through Ni; SC = Schaeffer (1971ApJ...163..411S) WD = Ward (1985MNRAS.213...71W) WF = Wiese & Fuhr (1975JPCRD...4..263W) WM = Wiese & Martin (1980, NSRDS-NBS 68, Part.2, US Governement Printing Office, Washington) WS= Wiese, Smith & Glennon (1966, NSRDS-NBS 4, US Governement Printing Office, Washington) and Wiese, Smith & Miles (1969, NSRDS-NBS, D.C.: US Department of Commerce, National Bureau of Standards) --- W1 Equivalent width for HD 133029 0.1pm log(N/Ntot)1 Deduced abundance for HD 133029 number=2 N = number of atoms/volume of particular element Ntotal = number of atoms/volume of all elements --- W2 Equivalent width for HD 192913 0.1pm log(N/Ntot)2 Deduced abundance for HD 192913 number=2 N = number of atoms/volume of particular element Ntotal = number of atoms/volume of all elements --- Relative abundances El Element --- log(El/Ntot)1 Elemental abundance for HD 133029 number=1 El = Element Ntot = number of atoms/volume of all elements --- e_log(El/Ntot)1 rms uncertainty on log(El/Ntot)1 --- log(El/Ntot)2 Elemental abundance for HD 192913 number=1 El = Element Ntot = number of atoms/volume of all elements --- e_log(El/Ntot)2 rms uncertainty on log(El/Ntot)2 --- table4.tex LaTeX version of table4 Patricia Bauer CDS 1999 Feb 19 Saul J. Adelman <ADELMANS@adelvx.citadel.edu> J_A+AS_137_227.xml Absolute declinations with the photoelectric astrolabe at Calern Observatory (OCA) J/A+AS/137/269 J/A+AS/137/269 Calern Observatory absolute declinations Absolute declinations with the photoelectric astrolabe at Calern Observatory (OCA) V A F Martin N V Leister G Vigouroux M Furia A Journet Astron. Astrophys. Suppl. Ser. 137 269 1999 1999A&AS..137..269M I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Fundamental catalog Positional data astrometry catalogs reference systems A regular observational programme with a photoelectric astrolabe have been performed at ``Observatoire du Calern" (Observatoire de la Cote d'Azur, OCA, {phi}=+43{deg}44'55.011"; {lambda}=-0^h^27^m^42.44^s^, Calern, Caussols, France) for the last twenty years. It has been almost fully automatized between 1984 and 1987. Since 1988 the photoelectric astrolabe was used without any modification. In addition to determining the daily orientation of the local vertical, the yearly analysis of the residuals permits to derive corrections to the used star catalogue Vigouroux et al. (1992A&AS...96..477V). A global reduction method was applied for the ASPHO observations. The new form of the equations Martin & Leister (1997A&AS..126..169M) give us the possibility of using the entire set of the observing program using data taken at two zenith distances (30{deg} and 45{deg}). The program contains about 41648 stars' transits of 269 different stars taken at ``Observatoire du Calern" (OCA). The reduction was based on the HIPPARCOS system. We discuss the possibility of computing absolute declinations through stars belonging simultaneously to the 30{deg} and 45{deg} zenith distances programmes. The absolute declination corrections were determined for 185 stars with precision of 0.027" and the value of the determined equator correction is -0.018"+/-0.005". The instrumental effects were also determined. The mean epoch is 1995.29.
Absolute declinations HIP HIPPARCOS (Cat. <I/239>) star number --- Vmag Visual magnitude mag B-V B-V colour index mag RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec DRA Position correction of right ascension (DRAcosDE) mas e_DRA rms uncertainty on DRA mas DDE Position correction of absolute declination mas e_DDE rms uncertainty on DDE mas HJD Heliocentric Julian Date of the observation d Patricia Bauer CDS 1999 May 04 Vera Martin <vmartin@cascavel.uefs.br> J_A+AS_137_269.xml Search for reference A0 dwarf stars: masses and luminosities revisited with Hipparcos parallaxes J/A+AS/137/273 J/A+AS/137/273 Reference A0V stars Search for reference A0 dwarf stars: masses and luminosities revisited with Hipparcos parallaxes M Gerbaldi R Faraggiana R Burnage F Delmas A E Gomez S Grenier Astron. Astrophys. Suppl. Ser. 137 273 1999 1999A&AS..137..273G I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) V/50 : Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991) J/ApJS/99/135 : Rotation and Spectral Peculiarities (Abt+ 1995) J/A+AS/122/51 : B to G stars calibration in Geneva photometry (Kunzli+, 1997) Parallaxes, trigonometric Photometry, uvby, beta Stars, A-type Stars, dwarfs Hertzsprung-Russell (HR diagram) stars: early-type stars: fundamental parameters Hipparcos data for 71 nearby dwarf A0 stars were combined with other data, in particular with high resolution spectra to establish the HR diagram in this temperature range. Almost 30% of unknown binaries were detected and discarded before establishing the M-L relation for bright A0 V field stars. The relationship derived for these single stars is compared to the classical diagram derived from eclipsing binaries. The scatter of the latter is examined and the role of gravity is discussed. A good agreement is found between the evolution-based surface gravity logg_ev_ and the value of logg_ph_ obtained from photometric data.
The programme stars HD HD (Cat. <III/135>) number --- HR HR (Cat. <V/50>) number --- SpType Spectral Type (BSC, Cat. <V/50>) number=1 When *, the note in the column Remarks concern the spectral type --- SpType2 Spectral type (Abt and Morrell, 1995, Cat. <J/ApJS/99/135>) --- Dmag Magnitude difference (BSC, Cat. <V/50>) --- Sep Angular separation (BSC, Cat. <V/50>) arcsec Bin Binarity by speckle arcsec n_Bin n: no detection, *: see Remarks column --- l_Vrot Limit flag on Vrot --- Vrot Rotational velocity (BSC, Cat. <V/50>) km/s l_Vrot2 Limit flag on Vrot2 --- Vrot2 Rotational velocity (Abt and Morrell, 1995, Cat. <J/ApJS/99/135>) km/s u_Vrot2 Uncertainty flag on Vrot2 --- Rem Remarks --- Photometric, astrometric data and atmospheric parameters HD HD (Cat. <III/135>) number --- b-y (b-y) color from uvbyBeta photometric system mag m1 m1 index from uvbyBeta photometric system mag c1 c1 index from uvbyBeta photometric system mag beta Beta from uvbybeta photometric system mag Group Group number for program UVBYBETA (Moon, 1985Ap&SS.117..261M) --- E(b-y) Reddening E(b-y) mag Teff Teff from Moon and Dworetsky (1985MNRAS.217..305M) calibration K logg log g from Moon and Dworetsky (1985MNRAS.217..305M) calibration [cm/s2] Teff2 Teff from Kunzli et al. (1997, Cat. <J/A+AS/122/51>) calibration K logg2 log g from Kunzli et al. (1997, Cat. <J/A+AS/122/51>) calibration [cm/s2] l_Broad Limit flag on Broad --- Broad Broadening value or lower value if interval km/s --- --- Broad2 Upper broadening value when interval km/s plx Parallax from Hipparcos (Cat. <I/239>) mas e_plx Relative error on the parallax from Hipparcos Catalogue (Cat. <I/239>) mas VMAG Absolute magnitude Mv mag e_VMAG Error on Mv mag HIP HIP (Cat. <I/239>) number --- Summary of the spectral analysis HD HD (Cat. <III/135>) number --- Cross Comments on the cross correlation curve --- Hgamma Comments on the comparison between observed and computed Hgamma profile --- MgII Comments on the comparison between observed and computed MgII profile --- metal Comments on the comparison between observed and computed metal lines --- Rem Remarks --- Parameters computed from the HR diagram and evolutionary tracks for the reduced sample HD HD (Cat. <III/135>) number --- logL Logarithm of the star luminosity [solLum] e_logL Error on the log L [solLum] Mass Mass of the star solMass e_Mass Error on the mass solMass Rad Radius of the star solRad logg(ev) Gravity surface calculated with the mass determined with stellar evolution models [cm/s2] e_logg(ev) Error on logg(ev) [cm/s2] logAge Logarithm of the age [yr] e_logAge Error on the age % HIP HIP (Cat. <I/236>) number --- Patricia Bauer CDS 1999 Apr 06 Michele Gerbaldi <gerbaldi@iap.fr> J_A+AS_137_273.xml A visual survey for small non-stellar objects in the galactic plane on POSS II. Results of nineteen fields at 115{deg}<l<157{deg} J/A+AS/137/293 J/A+AS/137/293 ZOAG galaxies in 115{deg}<l<157{deg} A visual survey for small non-stellar objects in the galactic plane on POSS II. Results of nineteen fields at 115{deg}<l<157{deg} R Weinberger M Gajdosik C Zanin Astron. Astrophys. Suppl. Ser. 137 293 1999 1999A&AS..137..293W J/A+AS/110/269 : Galaxies in the "zone of avoidance". I. (Weinberger+, 1995) J/A+AS/117/1 : Galaxies in the "zone of avoidance". II. (Seeberger+, 1996) J/A+AS/117/369 : Galaxies in the "zone of avoidance". III. (Lercher+, 1996) J/A+AS/126/247 : Galaxies in the "zone of avoidance". IV. (Saurer+, 1997) J/A+AS/127/101 : Galaxies in the "zone of avoidance". V. (Seeberger+ 1998) Cross identifications Galaxy catalogs catalogs dust, extinction Galaxy: structure A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.
The catalog ZOAG ZOAG G Galaxy designation --- RA1950h Right ascension (1950) h RA1950m Right ascension (1950) min RA1950s Right ascension (1950) s DE1950- Declination sign (1950) --- DE1950d Declination (1950) deg DE1950m Declination (1950) arcmin DE1950s Declination (1950) arcsec RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign (2000) --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Dmaj maximum diameter on red film arcmin Dmin minimum diameter on red film arcmin CrossID cross ident with NED and SIMBAD number=1 NOTES02 and NED02 are taken from NED --- table2.tex LaTeX version of table2 Patricia Bauer CDS 1999 Apr 19 Caterina Zanin <caterina.zanin@uibk.ac.at> J_A+AS_137_293.xml The Hamburg/SAO Survey for Emission-Line Galaxies. II. The Second List of 128 Galaxies J/A+AS/137/299 J/A+AS/137/299 Hamburg/SAO Survey for ELGs. II. The Hamburg/SAO Survey for Emission-Line Galaxies. II. The Second List of 128 Galaxies S A Pustilnik D Engels A V Ugryumov V A Lipovetsky H -J Hagen A Yu Kniazev Yu I Izotov G Richter Astron. Astrophys. Suppl. Ser. 137 299 1999 1999A&AS..137..299P J/A+AS/135/511 : The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999) Galaxies, spectra Magnitudes Radial velocities Redshifts galaxies: compact galaxies: distances and redshifts galaxies: starburst surveyss We present the second part of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. In this paper we present new results of spectroscopy obtained with the 6m Russian telescope. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000A) and the presence of strong or moderate emission lines close to 5000A recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16 - 19.5. No other criteria were applied. The spectroscopy resulted in detection and quantitative spectral classification of 134 emission-line objects. For 121 of them the redshifts are determined for the first time. For 13 ELGs known before emission line ratios are presented at first time. 108 of 134 emission-line objects are classified as BCG/HII galaxies and 6 probable BCGs, 6 as QSOs, 1 as Seyfert galaxy, 1 as super-association in a dwarf spiral galaxy, 2 as probable LINERs, 14 are low excitation objects - either of starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxy (DANS) type -, and 1 nonclassified. 23 galaxies did not show significant emission lines. The five most metal-deficient BCGs discovered have oxygen abundances log(O/H)+12 in the range 7.4 to 7.7, similar to the most metal-deficient BCGs known before.
Coordinates, velocities, magnitudes and classification of emission-line galaxies Name Object name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec HRV Heliocentric radial velocity km/s e_HRV Error of radial velocity km/s Bmag Magnitude in B filter mag BMAG Absolute B-magnitude number=1 Absolute magnitudes are not corrected for the Galaxy extinction. mag Type Classification number=2 Only rough classification was done due to low S/N spectra. Spectral classification follows Salzer et al. (1989ApJS...70..479S) --- Names Other names from NED --- Coordinates, redshifts and magnitudes of QSOs Name Object name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec z Observed redshift --- Bmag Magnitude in B filter mag --- Detected emission lines --- Parameters of emission lines of galaxies Name Object name --- Note1 Note on observation number=1 '*': Objects observed under poor photometric conditions --- Note2 Note on H{alpha} number=2 '+': Parameters for H{alpha} line --- FHb Observed flux in H{beta}}4861{AA} emission line number=3 Absolute observed fluxes are given in 10^-16 erg/sec/cm^2 10-19W/m2 u_FHb Uncertainty flag on F4861 number=4 ':': Parameters with less confident values --- F[OII]/Hb Emission line fluxes ratio [OII]3727{AA}/H{beta} --- u_F[OII]/Hb Uncertainty flag on F[OII]/Hb number=4 ':': Parameters with less confident values --- F[OIII]/Hb Emission line fluxes ratio [OIII]5007{AA}/H{beta} --- u_F[OIII]/Hb Uncertainty flag on [OIII]/Hb number=4 ':': Parameters with less confident values --- FHa/Hb Emission line fluxes ratio H{alpha}/H{beta} --- u_FHa/Hb Uncertainty flag on FHa/Hb number=4 ':': Parameters with less confident values --- F[NII]/Ha Emission line fluxes ratio [NII]6583{AA}/H{alpha} --- F[SII]/Ha Emission line fluxes ratio [SII](6716A+6730{AA})/H{alpha} --- W3727 Equivalent width of [OII]3727{AA} emission line 0.1nm u_W3727 Uncertainty flag on W3727 number=4 ':': Parameters with less confident values --- n_W3727 Note on W3727 number=2 '+': Parameters for H{alpha} line --- W4861 Equivalent width of Hb emission line 0.1nm u_W4861 Uncertainty flag on W4861 number=4 ':': Parameters with less confident values --- W5007 Equivalent width of [OIII]5007{AA} emission line 0.1nm Galaxies without emission lines Name Object name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec HRV Heliocentric radial velocity km/s u_HRV Uncertainty flag on HRV number=1 ':': Parameters with less confident values --- Bmag Magnitude in B filter mag BMAG Absolute B-magnitude number=2 Absolute magnitudes are not corrected for the Galaxy extinction. mag ALine Absorption lines --- Star positions and spectral features Name Object name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Bmag Magnitude in B filter mag Type Spectral type of a star --- Lines Spectral features --- tables.tex LaTeX version of the tables tables.ps PostScript version of the tables Patricia Bauer CDS 1999 Apr 06 Simon A. Pustilnik <sap@sao.ru> J_A+AS_137_299.xml IC 348 proper motion study from digitised Schmidt plates. J/A+AS/137/305 J/A+AS/137/305 IC 348 proper motion catalogue IC 348 proper motion study from digitised Schmidt plates. R -D Scholz J Brunzendorf G Ivanov N Kharchenko B Lasker H Meusinger T Preibisch E Schilbach H Zinnecker Astron. Astrophys. Suppl. Ser. 137 305 1999 1999A&AS..137..305S I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) I/246 : The ACT Reference Catalog (Urban+ 1997) I/146 : Positions and Proper Motions - North (Roeser+, 1988) Clusters, open Photometry Proper motions astrometry methods: statistical open clusters and associations: individual: IC 348 stars: kinematics A new proper motion study for about 1400 stars with R<18mag in a one square degree region around the young open cluster IC 348 based on Schmidt plates is presented. With an overall accuracy of about 3mas/yr (2.5mas/yr, respectively for all stars with R<17mag) we have obtained membership probabilities dividing our sample into three groups: foreground stars, cluster stars and background stars. This separation is also supported by the proper motion distribution with respect to the direction of the standard antapex and an increase of mean proper motion cluster membership probabilities with smaller cluster radii. 240 stars of our sample have cluster membership probabilities larger than 80%.
IC 348 catalogue of proper motions Seq Sequential number number=1 Original number in a larger sample of all objects detected on the reference plate. --- RAh Right ascension (J2000, Epoch=1955.81) number=2 The coordinates are given for equinox J2000 but with the epoch of the reference plate e1457 (i.e. 1955.81). h RAm Right ascension (minutes) number=2 The coordinates are given for equinox J2000 but with the epoch of the reference plate e1457 (i.e. 1955.81). min RAs Right ascension (seconds) number=2 The coordinates are given for equinox J2000 but with the epoch of the reference plate e1457 (i.e. 1955.81). s DE- Declination sign number=2 The coordinates are given for equinox J2000 but with the epoch of the reference plate e1457 (i.e. 1955.81). --- DEd Declination (J2000, Epoch=1955.81) number=2 The coordinates are given for equinox J2000 but with the epoch of the reference plate e1457 (i.e. 1955.81). deg DEm Declination (arcminutes) number=2 The coordinates are given for equinox J2000 but with the epoch of the reference plate e1457 (i.e. 1955.81). arcmin DEs Declination (arcseconds) number=2 The coordinates are given for equinox J2000 but with the epoch of the reference plate e1457 (i.e. 1955.81). arcsec pmRA Proper motion mu_alpha.cos(delta) mas/yr pmDE Proper motion mu_delta mas/yr e_pmRA rms uncertainty on pmRA mas/yr e_pmDE rms uncertainty on pmDE mas/yr U9167 U9167 magnitude mag B9168 B9168 magnitude mag B9177 B9177 magnitude mag Bj Bj magnitude mag Vmag V magnitude mag Emag E magnitude mag Rmag R magnitude mag Pcl Membership probability of the cluster IC 348 % Pdf Membership probability of the group of distant field stars % Patricia Bauer CDS 1999 Aug 16 Ralf Scholz <rdscholz@aip.de> J_A+AS_137_305.xml Understanding A-type supergiants. I. Ultraviolet and visible spectral atlas of A-type supergiants J/A+AS/137/351 J/A+AS/137/351 A supergiants UV and visible spectra Understanding A-type supergiants. I. Ultraviolet and visible spectral atlas of A-type supergiants E Verdugo A Talavera A I Gomez de Castro Astron. Astrophys. Suppl. Ser. 137 351 1999 1999A&AS..137..351V Atlases Spectra, ultraviolet Stars, supergiant atlases line: profiles supergiants ultraviolet: stars This paper is the first of a series whose aim is to perform a systematic study of A-type supergiant atmospheres and winds. Here we present a spectral atlas of 41 A-supergiants observed by us in high and medium resolution in the visible and ultraviolet. The atlas consists of profiles of the H{alpha}, H{beta}, H{gamma}, H{delta}, H{epsilon}, Ca II (H and K), Na I (D1 and D2), Mg II_4481_, Mg II [uv1] and Fe II [uv1, uv2, uv3, uv62, uv63, uv161] lines for 41 stars with spectral types ranging from B9 to A9 and luminosity classes Ia, Iab and Ib, and provides the basic data for a thoughtful study of these stars. The overall characteristics of the sample as well as the data reduction procedures are described. We also present some examples of spectral variability.
Basic properties of the program stars HD/BD HD (Cat. <III/135>) or BD (Cat. <I/122>) name --- Name Other name --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign (2000.0) --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec Vmag Visual magnitude mag VMAG Absolute visual magnitude mag OB OB association name --- Visible Observed (Y) or not observed (N) in visible --- IUE Observed (Y) or not observed (N) in IUE --- fig1 Name of the figure containing the spectrum --- fig2 Name of the figure containing the spectrum --- fig3 Name of the figure containing the spectrum --- tables.tex LaTeX version of tables 1 to 8 Patricia Bauer CDS 1999 Apr 22 Eva Verdugo Rodrigo <everdugo@iso.vilspa.esa.es> J_A+AS_137_351.xml Orbital elements and physical parameters of ten chromospherically active binary stars J/A+AS/137/369 J/A+AS/137/369 10 active binary radial velocities Orbital elements and physical parameters of ten chromospherically active binary stars C Fekel K G Strassmeier M Weber A Washuettl Astron. Astrophys. Suppl. Ser. 137 585 1999 1999A&AS..137..369F V/76 : Chromospherically Active Binaries (Strassmeier+ 1993) Binaries, spectroscopic Radial velocities binaries: general binaries: spectroscopic stars: activity stars: fundamental parameters stars: late-type Orbital elements have been determined for 10 chromospherically active binaries from a combination of new velocities and velocities in the literature. First orbits for three binaries, HD 33363, HD 152178, and HD 208472, are presented, as well as updated orbits for seven other binaries. Two of the latter systems, LN Peg and HD 106225 were discovered to be triple, and both short- and long-period orbits have been computed for each. Fundamental properties have been determined for the chromospherically active primary in each system.
LN Peg 00 12 30.3 +14 33 48 zeta And 00 47 20.3 +24 16 02 HD 33363 05 18 31.1 +75 56 49 HD 81410 09 24 49.0 -23 49 34 HU Vir A HD 106225 12 13 20.7 -09 04 47 HD 136901 15 22 25.3 +25 37 27 UZ Lib 15 32 23.2 -08 32 01 HD 152178 16 52 56.0 -26 45 02 HD 208472 21 55 14.5 +44 25 07 IM Peg HD 216489 HR 8703 22 53 02.3 +16 50 28
Radial velocities (tables A1 to A15) Star Star name number=1 LN Peg Aa: = BD 1313 Aa, velocities for Aa constructed with general least-squares program LN Peg Ab: = BD 13 13Ab, velocities of Ab constructed with general least-squares program zeta And: National Solar Observatory (NSO) & Kitt Peak National Observatory (KPNO) final circular orbit fit HD 33363: Fekel & Vienna velocities from KPNO HD 81410A: Circular orbit fit for Tables HD 81410B: Circular orbit fit for Tables HD 106225: Constructed short-period velocities from general least-squares program long period velocities from general least-squares program HD 136901: orbital solution table UZ Lib: KPNO coude, circular orbit HD 152178: RVs (corrected for spectral type missmatch & reduced prog) Vienna added HD 208472: all Fekel and Vienna Radial velocities: Circular Orbit HR 8703: Vienna and Demp KPNO, Harper & Demp NSO, final circular orbit --- RVPer l: long-period velocity s: short-period velocity --- HJD Heliocentirc Julian date d Phase Phase computed from the orbital elements in table5.dat file --- RV Observed radial velocity km/s RV(O-C) Residual velocities from the computed orbit km/s w_RV Assigned statistical weight --- r_RV Source code for radial velocities number=2 ESO: ESO, 1996 KFA: KNPO, 1982 KPNO: KNPO KF: KNPO, 1995-98 KR: KPNO, 1982-83 KT1: KNPO, 1983-87 KT2: KNPO, 1987-98 MR: McDonald, 1979-81 NSO: NSO, 1996-97 Dadonas: Dadonas, 1994, Priv. comm. Donati: Donati et al., 1997MNRAS.291..658D Fleming: Fleming et al., 1989AJ.....98..692F Harper: Harper, 1920PDAO....1..203H, 1935PDAO....6..207H Latham: Latham et al., 1988AJ.....96..567L Olah: 1998A&A...330..559O --- Orbital elements Star Star name --- Porb Orbital period d e_Porb rms uncertainty on Porb d T0 Time of maximum positive velocity d e_T0 rms uncertainty on T0 d Tperi Time of perihelion passage d e_Tperi rms uncertainty on Tperi d v0 System's center-of-mass radial velocity km/s e_v0 rms uncertainty on v0 km/s K Semiamplitude of the hot/cool component --- e_K rms uncertainty on K --- e Eccentricity --- e_e rms uncertainty on e --- omega Longitude of perihelion deg e_omega rms uncertainty on omega deg asini Separation a sin(i) for hot/cool number=1 If single lined, a_1_*sini; if double lined, both semi-major axes are given. 10+6km e_asini rms uncertainty on asini 10+6km f(m) Mass function number=2 If double lined, m*sin^3^ i is listed. solMass e_f(m) rms uncertainty on f(m) solMass Patricia Bauer CDS 1999 Apr 27 Klaus G. Strassmeier <STRASSMEIER@asrael.ast.univie.ac.at> J_A+AS_137_369.xml Dynamics of blue compact galaxies as revealed by their H-alpha velocity fields. I. The data, velocity fields and rotation curves. J/A+AS/137/419 J/A+AS/137/419 Dynamics of blue compact galaxies I. The data Dynamics of blue compact galaxies as revealed by their H-alpha velocity fields. I. The data, velocity fields and rotation curves. G Oestlin P Amram J Masegosa N Bergvall J Boulesteix Astron. Astrophys. Suppl. Ser. 137 419 1999 1999A&AS..137..419O Galaxies, rotation Rotational velocities galaxies: compact galaxies: interactions galaxies: ISM galaxies: kinematics and dynamics galaxies: starburst Observations of six luminous blue compact galaxies (BCGs) and two star forming companion galaxies were carried out with the CIGALE scanning Fabry-Perot interferometer attached to the ESO 3.6m telescope on La Silla. The observations were made in the H-alpha emission line which is prominent in BCGs. A velocity sampling of 5km/s and a pixel size of 0.9arcseconds were used. In this paper we present the observations and the data together with the velocity fields and the derived rotation curves. In addition we provide rough estimates of the total dynamical mass and of the ionised gas mass for each galaxy. All galaxies display rotation, but while the companion galaxies have regular velocity fields, those of the BCGs are complex and appear perturbed. This is the most extensive study to date of the optical velocity fields of BCGs. The interpretation of these results will be presented in a forthcoming paper (Paper II).
Rotation curves Name Galaxy name --- Model Model version number=1 Some galaxies have been modelled in different ways, e.g. decomposing the velocity field (VF) into two components. When present the label Model indicates which model the rotation curve (RC) refers to. Total = RC built from the non decomposed velocity field 1st = RC built from the first component of the decomposed VF 2nd = RC built from the second component of the decomposed VF Main = RC built from the main component of the non decomposed VF FP1 = RC built from observations with Fabry-Perot interferometer 1 Masked = RC built after masking points in the non decomposed VF East = RC refers to the first component of the eastern galaxy West = RC refers to the first component of the western galaxy For further explanations of the different models see paper. --- Rad Mean radius of the annulus on the major axis arcsec o_Vapp Number of points for the approaching side number=2 The number of velocity points included in calculating the velocity at the given radius --- Vapp Weighted average velocity for approaching side km/s e_Vapp rms uncertainty on Vapp km/s o_Vrec Number of points for the receding side number=2 The number of velocity points included in calculating the velocity at the given radius --- Vrec Weighted average velocity for receding side km/s e_Vrec rms uncertainty on Vrec km/s o_Vtot Total Number of points = o_Vapp + o_Vrec --- Vtot Weighted average velocity for both sides km/s e_Vtot rms uncertainty on Vtot km/s Patricia Bauer CDS 1999 Feb 25 Goran Ostlin <ostlin@iap.fr> J_A+AS_137_419.xml OH and H2O masers in 74 star-forming regions. The FC89 database J/A+AS/137/43 J/A+AS/137/43 OH/H2O masers database OH and H2O masers in 74 star-forming regions. The FC89 database J R Forster J L Caswell Astron. Astrophys. Suppl. Ser. 137 43 1999 1999A&AS..137...43F H II regions Masers Radial velocities Radio lines catalogs HII regions masers stars: pre-main sequence Table 3 contains VLA spectra and positions for OH and H2O maser spots in 74 star-forming regions mapped by Forster and Caswell (1989A&A...213..339F). Galactic coordinates are given, followed by offset positions of the 22GHz continuum peak (HII) if detected, and the flux, velocity and positions of OH and H_2_O maser spots mapped in that field.
Field positions Field Designation by galactic coordinates --- RAh Field-center right ascension (1950) h RAm Field-center right ascension (1950) min RAs Field-center right ascension (1950) s DE- Field-center declination sign (1950) --- DEd Field-center declination (1950) deg DEm Field-center declination (1950) arcmin DEs Field-center declination (1950) arcsec FC89 - OH/H2O maser VLA database Field Designation by galactic coordinates --- Maser HII, OH or H2O --- S OH (1665MHz) or H2O (23235MHz) flux density (in Jy/beam) Jy RV LSR radial velocity km/s oRA Offset in right ascension from reference position (in object.dat file) arcsec oDEC Offset in declination from reference position (in object.dat file) arcsec Patricia Bauer CDS 1999 Apr 22 Rick Forster <rick@bima.Astro.uiuc.EDU> J_A+AS_137_43.xml Radial velocities. IX. Measurements of 2800 B2-F5 stars for Hipparcos J/A+AS/137/451 J/A+AS/137/451 Radial velocities. IX. Radial velocities. IX. Measurements of 2800 B2-F5 stars for Hipparcos S Grenier M O Baylac L Rolland R Burnage F Arenou D Briot F Delmas M Duflot V Genty A E Gomez J -L Halbwachs M Marouard E Oblak A Sellier Astron. Astrophys. Suppl. Ser. 137 451 1999 1999A&AS..137..451G I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) III/163 : Fourth cat. of Am stars with known sp. types (Hauck, 1992) I/211 : CCDM, Comp. of Double and Multiple stars (Dommanget+ 1994) III/190 : WEB Catalog of Radial Velocities (Duflot+ 1995) J/A+AS/135/503 : Hipparcos southern B8-F2 stars RV (Grenier+ 1999) J/A+AS/110/177 : Mesure de vitesses radiales. VII. (Duflot+, 1995) J/A+AS/124/255 : Radial velocities measurements. VIII. (Duflot+ 1997) Fehrenbach et al. Paper I. 1987A&AS...71..263F Fehrenbach et al. Paper II. 1987A&AS...71..275F Fehrenbach & Burnage Paper III. 1990A&AS...83...91F Duflot et al. Paper IV. 1990A&AS...83..251D Duflot et al. Paper V. 1992A&AS...94..479D Fehrenbach et al. Paper VI. 1992A&AS...95..541F Duflot et al. Paper VII. 1995A&AS..110..177D, Cat. <J/A+AS/110/177> Duflot et al. Paper VIII 1997A&AS..124..255F, Cat. <J/A+AS/124/255> Radial velocities Stars, early-type stars: early-type stars: fundamental parameters techniques: radial velocities Radial velocities have been determined for a sample of 2930 B2-F5 stars, 95% observed by the Hipparcos satellite in the north hemisphere and 80% without reliable radial velocity up to now. Observations were obtained at the Observatoire de Haute Provence with a dispersion of 80{AA}/mm with the aim of studying stellar and galactic dynamics. Radial velocities have been measured by correlation with templates of the same spectral class. The mean obtained precision is 3.0km/s with three observations. A new MK spectral classification is estimated for all stars.
Radial velocities of Hipparcos Catalogue stars --- Catalogue abbreviation --- HIP HIP (Cat. <I/239>) number --- HD/BD HD (Cat. <III/135>) or BD (Cat. <I/122>) number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag r_Vmag Source of magnitude number=1 H: Hipparcos (Cat. <I/239>) magnitude Hp and a colour index G: ground-based photometry T: Tycho (Cat. <I/239>) photometry --- SpType Spectral type --- n_SpType R if the luminosity class is not consistent with Hipparcos parallax. (See table6.dat) --- KNO H if the star belongs to the fourth Catalogue of Am Stars with known spectral types (Hauck, Cat. <III/163>) --- SpTypeAd Adopted spectral type --- RV Mean radial velocity km/s e_RV Error on radial velocity km/s o_RV Number of observations --- Var Variability indication --- E/I Ratio E/I of external to internal error --- n_RV P if the radial velocity replaces the one published already in Paper I (Fehrenbach et al., 1987A&AS...71..263F) --- Time T if the observation time is <214 days, t if it is between 214 and 305 days --- u_RV C when a secondary component (separation <2.0" and magnitude difference <1mag) can disturb the radial velocity c idem with the data coming from CCDM (Cat. <I/221>) --- Note flag on the Hipparcos photometry number=2 C: constant D: duplicity M: possibly micro-variable P: periodic variable R: revised (V-I) colour index U: unsolved variable --- Mult Number of astrometric components --- n_Mult double and multiple system flag about astrometry number=3 C: given solution (P>3.3 years generally if physical) O: orbital solution G: solution with acceleration term (unresolved system, probable P>10 years) V: variability of one of the components X: stochastic solution (possible binary with P <3 years) --- q_Mult solution quality flag number=4 A: good B: fair C: poor D: uncertain S: suspected non-single --- Comp Concerned components, the brightest being the first --- Sep Separation number=5 When Sep and dHp values have one decimal only they come from CCDM (Dommanget & Nys, 1994BICDS..45....7D, 1996, Cat. <I/211>) arcsec dHp Difference of magnitude dHp number=5 When Sep and dHp values have one decimal only they come from CCDM (Dommanget & Nys, 1994BICDS..45....7D, 1996, Cat. <I/211>) mag CCDM * when CCDM (Cat. <I/221>) gives a complementary information about secondary component(s) --- O O: astrometric orbit in CCDM (Cat. <I/221>) --- Radial velocities of stars out of the Hipparcos Catalogue (Cat. <I/239>) HD/BD HD (Cat. <III/135>) or BD (Cat. <I/122>) number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag r_Vmag Source of magnitude (C: CDS) --- SpType Spectral type --- KNO H if the star belongs to the fourth Catalogue of Am Stars with known spectral types (Hauck, Cat. <III/163>) --- SpTypeAd The adopted spectral type --- RV Mean radial velocity km/s e_RV Error on radial velocity km/s o_RV Number of observations --- Var Variability indication --- E/I Ratio E/I of external to internal error --- n_RV P if the radial velocity replaces this published already in Paper I (Fehrenbach et al., 1987A&AS...71..263F) --- Time T if the observation time is < 214 days t if it is between 214 and 305 days --- u_RV c when a secondary component (separation <2.0" and dmv<1mag in CCDM, Cat. <I/221>) can disturb the radial velocity --- CCDM * when the star is in CCDM (Cat. <I/221>) --- Stars with a discrepancy between the luminosity classes given by visual classification and by Hipparcos parallax --- Catalogue abbreviation --- HIP HIP (Cat. <I/239>) number --- HD/BD HD (Cat. <III/135>) or BD (Cat. <I/122>) number --- SpType Visual spectral type --- Class Luminosity class given by the Hipparcos parallax --- Note Notes number=1 1: probable overestimate absorption 2: probable underestimate absorption 3: binary with separation <1.2" and magnitude difference <2 4: variable radial velocity or suspected binary by Hipparcos 5: error on absolute magnitude >2mag --- Patricia Bauer CDS 1999 May 27 Suzanne Grenier <Suzanne.Grenier@obspm.fr> J_A+AS_137_451.xml An H{alpha} catalogue of galaxies in Hickson Compact Groups. I. The Sample J/A+AS/137/495 J/A+AS/137/495 Halpha Catalogue of HCG Galaxies An H{alpha} catalogue of galaxies in Hickson Compact Groups. I. The Sample P Severgini B Garilli P Saracco G Chincarini Astron. Astrophys. Suppl. Ser. 137 495 1999 1999A&AS..137..495S VII/213 : Hickson Compact Groups of Galaxies (Hickson 1982) Galaxies, photometry Photometry, H-alpha galaxies: clusters: general galaxies: evolution galaxies: interactions We present H{alpha} photometry for a sample of 95 galaxies in Hickson Compact Groups (Cat. <VII/213>) obtained from observations of 31 groups. The Catalogue lists isophotal and adaptive aperture (Kron aperture) flux measurements for about 75% of the accordant galaxies inside the observed HCGs, 22 out of which are upper limits. Non standard data reduction procedures have been used to obtain the continuum subtracted H{alpha} images for each HCG of the target sample. Flux calibration has also been performed in order to obtain H{alpha} luminosities for the whole sample. Both the data reduction and calibration procedures are carefully described in the paper.
Galaxy positions HCG Hickson galaxy designation --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec H{alpha} isophotal Fluxes and Luminosities HCG Hickson galaxy designation --- F1 Flux uncorrected for galactic and internal extinction 10-13mW/m2 e_F1 Error on F1 10-14mW/m2 L1 Luminosity uncorrected for galactic and internal extinction (10^38^erg/s) 10+31W e_L1 Error on L1 10+31W F2 Flux corrected for galactic extinction 10-13mW/m2 e_F2 Error on F2 10-14mW/m2 F3 Flux corrected for Galactic and internal extinction number=1 Values of -1.00 indicate that the galaxies is not a spiral galaxy and the value of F3 is not needed for it 10-13mW/m2 Area Isophotal area arcsec+2 S/N Signal to noise ratio --- Isophotal corrected and Kron fluxes HCG Hickson galaxy designation --- Fisocor Isophotal corrected flux 10-13mW/m2 e_Fisocor Error on fisocor 10-14mW/m2 Fkron =-1.00 Kron flux 10-13mW/m2 e_Fkron =-1.00 Error on fkron 10-14mW/m2 Upper limits to flux and luminosity HCG Hickson galaxy designation --- Fup Flux at 3{sigma} from bkg 10-13mW/m2 e_Fup Error on Fup 10-14mW/m2 Lup Luminosity at 3{sigma} 10+31W e_Lup Error on Lup 10+31W Patricia Bauer CDS 1999 May 18 Paola Severgnini <paolas@arcetri.astro.it> J_A+AS_137_495.xml High resolution spectroscopy over lambda 8500-8750{AA}. I. Mapping the MKK classification system. J/A+AS/137/521 J/A+AS/137/521 8500-8750{AA} high resolution spectroscopy High resolution spectroscopy over lambda 8500-8750{AA}. I. Mapping the MKK classification system. U Munari L Tomasella Astron. Astrophys. Suppl. Ser. 137 521 1999 1999A&AS..137..521M http://ulisse.pd.astro.it/Astro/Atlases/ : spectra of stars listed in table2 Atlases MK spectral classification Rotational velocities atlases standards stars: fundamental parameters We present an Echelle+CCD high resolution spectroscopic atlas mapping the MKK classification system over the wavelength interval lambda 8500-8750 A, centered on the near-IR triplet of Ca II. Table 2 lists all the 131 program stars with basic informations (magnitudes, coordinates, spectral types, metallicities, rotational velocities, variabilities) and the journal of observations; Table 3 shows our mapping of the MKK scheme in terms of spectral and luminosity classes; Table 4 lists the major un-blended absorption lines which we identified in our spectra
A List of atlases covering this spectral region HD HD star number --- m_HD Multiplicity index on HD --- HIP Hipparcos star number --- Vmag Visual magnitude mag RAdeg Right ascension (J2000) deg DEdeg Declination (J2000) deg Spect Spectral type --- LumClass Luminosity class --- Source See Note number=1 YNN: Yamashita, Nariai and Norimoto (1977), University of Tokyo Press "An atlas of representative stellar spectra" w: Walborn (1973AJ.....78.1067W) g: Garcia (1989, Cat. <III/149>) l: Lang (1992), Springer-Verlag New York, Inc. gg: Gray and Garrison (1989ApJS...69..301G and 1989ApJS...70..623G) kmn: Keenan and McNeil (1989, Cat. <III/150>) j: Jaschek (1978, Cat. <III/42>) bsc: the Bright Star Catalogue, Hoffleit et al. (1991, Cat. <V/50>) --- [Fe/H] Metallicity [Sun] vsini Projected rotational velocity km/s cv Coarse variability from Hipparcos Catalogue --- var Variability type from Hipparcos Catalogue --- SB Spectroscopic binary type --- ExpTime Total exposition time s S/N Signal-to-noise ratio --- atlas Atlases which include the same stars number=2 m: Montes and Martin (1998, Cat. <J/A+AS/128/485>) a: Andrillat et al. (1995, Cat. <III/183>) s: Serote Roos et al. (1996, Cat. <J/A+AS/117/93>) k: Kiehling (1987, Cat. <III/124>) d: Danks and Dennefeld (1994PASP..106..382D) t: Torres-Dodgen and Weaver (1993, Cat. <III/181>) w: Weaver and Torres-Dodgen (1995, Cat. <J/ApJ/446/300>) --- Our mapping of the MKK scheme SpType Spectral type --- ClassI HD number for stars of luminosity class I --- m_ClassI Multiplicity index on HD number --- ClassII HD number for stars of luminosity class II --- ClassIII HD number for stars of luminosity class III --- ClassIV HD number for stars of luminosity class IV --- ClassV HD number for stars of luminosity class V --- m_ClassV Multiplicity index on HD number --- Identification of the main lines observed Ion Ion --- Lambda Wavelength 0.1nm Mult Multiplet number --- Mul2 Second multiplet number for double FeI multiplet --- Patricia Bauer CDS 1999 Apr 29 Lina Tomasella <tomasell@astras.pd.astro.it> J_A+AS_137_521.xml ESO Imaging Survey. IV. Multicolour analysis of point-like objects toward the South Galactic Pole. J/A+AS/137/75 J/A+AS/137/75 ESO Imaging Survey ESO Imaging Survey. IV. Multicolour analysis of point-like objects toward the South Galactic Pole. S Zaggia I Hook R Mendez L Da Costa L F Olsen M Nonino A Wicenec C Benoist E Deul T Erben M D Guarnieri R Hook I Prandoni M Scodeggio R Slijkhuis R Wichmann Astron. Astrophys. Suppl. Ser. 137 75 1999 1999A&AS..137...75Z Photometry, UBVRI QSOs Stars, white dwarf Surveys quasars: general stars: low-mass, brown dwarfs surveys white dwarfs This paper presents preliminary lists of potentially interesting point-like sources extracted from multicolour data obtained for a 1.7 square degree region near the South Galactic Pole. The region has been covered by the ESO Imaging Survey (EIS) in B, V and I and offers a unique combination of area and depth. These lists, containing a total of 330 objects nearly all brighter than I~21.5, over 1. 27 square degrees (after removing some bad regions), are by-products of the process of verification and quality control of the object catalogs being produced. Among the colour selected targets are candidate very low mass stars/brown dwarfs (54), white-dwarfs (32), and quasars (244). In addition, a probable fast moving asteroid was identified. The objects presented here are natural candidates for follow-up spectroscopic observations and illustrate the usefulness of the EIS data for a broad range of science and for providing possible samples for the first year of the VLT.
Very low-mass star candidates Very low-mass star candidates (B-dropout) Very low-mass star candidates (detected in I) White dwarfs candidates Quasar candidates Quasar candidates (B-dropout) Quasar candidates (low redshift) EIS EIS list designation --- Seq Sequence number in list --- RAh Right ascension hour (J2000.0) h RAm Right ascension minute (J2000.0) min RAs Right ascension second (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination degree (J2000.0) deg DEm Declination minute (J2000.0) arcmin DEs Declination second (J2000.0) arcsec Imag Magnitude I mag e_Imag Magnitude error on I mag l_(B-V) Limit flag on (B-V) --- (B-V) Magnitude colour (B-V) mag e_(B-V) Magnitude colour error on (B-V) mag l_(V-I) Limit flag on (V-I) --- (V-I) Magnitude colour on (V-I) mag e_(V-I) Magnitude colour error on (V-I) mag Notes Cross identification with NED and SIMBAD, redshift --- Patricia Bauer CDS 1999 Jun 11 J_A+AS_137_75.xml CCD astrometric observations of Uranian satellites: 1995-1998 J/A+AS/138/247 J/A+AS/138/247 Uranian satellites 1995-1998 CCD astrometric observations of Uranian satellites: 1995-1998 C H Veiga R Vieira Martins Astron. Astrophys. Suppl. Ser. 138 247 1999 1999A&AS..138..247V J/A+AS/107/559 : Position of Uranian satellites (Veiga+, 1994) J/A+AS/113/557 : Uranian satellites (Veiga+, 1995) Planets Positional data Solar system CCD astrometry planets and satellites: general planets and satellites: individual (satellites of Uranus) Astrometric positions of the five largest Uranian satellites from 750 CCD frames taken at the oppositions of 1995 through 1998 are presented. The images were obtained over 35 nights. Observed positions are compared with the calculated positions from GUST86. The standard deviations are better than 0.05" for the four largest satellites and 0.08" for Miranda.
List of observed positions of the Uranian satellites Year Year of observation --- Month Month of observation --- UTCday UTC day of observation d XposM Miranda X position referred to Oberon number=1 The reference system is defined by the mean equator and equinox J2000 X={Delta}RAcosDE; Y={Delta}DE arcsec YposM Miranda Y position referred to Oberon number=1 The reference system is defined by the mean equator and equinox J2000 X={Delta}RAcosDE; Y={Delta}DE arcsec XposA Ariel X position referred to Oberon number=1 The reference system is defined by the mean equator and equinox J2000 X={Delta}RAcosDE; Y={Delta}DE arcsec YposA Ariel Y position referred to Oberon number=1 The reference system is defined by the mean equator and equinox J2000 X={Delta}RAcosDE; Y={Delta}DE arcsec XposU Umbriel X position referred to Oberon number=1 The reference system is defined by the mean equator and equinox J2000 X={Delta}RAcosDE; Y={Delta}DE arcsec YposU Umbriel Y position referred to Oberon number=1 The reference system is defined by the mean equator and equinox J2000 X={Delta}RAcosDE; Y={Delta}DE arcsec XposT Titania X position referred to Oberon number=1 The reference system is defined by the mean equator and equinox J2000 X={Delta}RAcosDE; Y={Delta}DE arcsec YposT Titania Y position referred to Oberon number=1 The reference system is defined by the mean equator and equinox J2000 X={Delta}RAcosDE; Y={Delta}DE arcsec Patricia Bauer CDS 1999 Jun 18 Carlos Henrique Veiga <cave@obsn.on.br> J_A+AS_138_247.xml A search for candidate light echoes: photometry of supernova environments J/A+AS/138/253 J/A+AS/138/253 Supernova light echoes A search for candidate light echoes: photometry of supernova environments F R Boffi W B Sparks F D Macchetto Astron. Astrophys. Suppl. Ser. 138 253 1999 1999A&AS..138..253B Photometry, UBVRI Supernovae distance scale scattering supernovae: general Supernova (SN) light echoes could be a powerful tool for determining distances to galaxies geometrically, Sparks (1994ApJ...433...19S). In this paper we present CCD photometry of the environments of 64 historical supernovae, the first results of a program designed to search for light echoes from these SNe. We commonly find patches of optical emission at, or close to, the sites of the supernovae. The color distribution of these patches is broad, and generally consistent with stellar population colors, possibly with some reddening. However there are in addition patches with both unusually red and unusually blue colors. We expect light echoes to be blue, and while none of the objects are quite as blue in V-R as the known light echo of SN 1991T, there are features that are unusually blue and we identify these as candidate light echoes for follow-on observations.
JKT run photometry ESO run photometry Galaxy Galaxy designation --- Run Run specification --- SN Supernova designation --- Type Supernova Type number=1 The SN Type was taken from Branch (1990, in "Supernovae", Petschek A.G. (ed.), Springer-Verlag, pp. 39-42) and/or from the Sternberg Catalog (Cat. <II/218/>; ':' after a Type indicates that according to the Sternberg Catalog there is uncertainty; both Types are classified spectroscopically, but the Type II are also classified according to the shape of the light curve (P=plateau; L=linear) as given by the Sternberg Catalog. This means that whenever a Type II is indicated as a Type IIP or IIL the Sternberg classification was used; for some objects only the Sternberg classification Type is found and is indicated in parenthesis; for SNe 1940E and 1963L the two sources disagree: both are given. --- Patch Patch designation number=2 We list all patches that have been identified at (or close to) the site of the supernova and that were bright enough to be detected during the observation: they are numbered and briefly described by a comment that follows. Such features are close to/within a ring of approximately 5 arcsec in radius centered at the nominal position of the supernova (see Figs. 1 through 36). --- n_Patch Patch description --- xpos Patch x offset arcsec n_xpos --- ypos Patch y offset arcsec n_ypos --- Bmag Magnitude at 4400A mag n_Bmag Comment on B magnitude number=3 $: IRAF program ``phot'' did not calculate the magnitude in some band and thus the color could not be derived #: no images were taken in that band s: saturated near the nucleus --- Vmag Magnitude at 5000A mag n_Vmag Comment on V magnitude --- Rmag Magnitude at 6400A mag n_Rmag Comment on R magnitude number=3 $: IRAF program ``phot'' did not calculate the magnitude in some band and thus the color could not be derived #: no images were taken in that band s: saturated near the nucleus --- B-V B-V colour index mag V-R B-V colour index mag Blim Limiting magnitude at 4400A number=4 The limiting magnitudes correspond to a 5{sigma} detection, unless a flag * indicates a 3{sigma} detection mag n_Blim Comment on B limiting magnitude number=4 The limiting magnitudes correspond to a 5{sigma} detection, unless a flag * indicates a 3{sigma} detection --- Vlim Limiting magnitude at 5000A number=4 The limiting magnitudes correspond to a 5{sigma} detection, unless a flag * indicates a 3{sigma} detection mag n_Vlim Comment on V limiting magnitude number=4 The limiting magnitudes correspond to a 5{sigma} detection, unless a flag * indicates a 3{sigma} detection --- Rlim Limiting magnitude at 6400A number=4 The limiting magnitudes correspond to a 5{sigma} detection, unless a flag * indicates a 3{sigma} detection mag n_Rlim Comment on R limiting magnitude number=4 The limiting magnitudes correspond to a 5{sigma} detection, unless a flag * indicates a 3{sigma} detection --- e_Bmag Standard deviation in B mag e_Vmag Standard deviation in V mag e_Rmag Standard deviation in R mag Patricia Bauer CDS 1999 Jun 10 Francesca Boffi <boffi@stsci.edu> J_A+AS_138_253.xml Line identifications and intensities for the optical spectrum of RR Telescopii between 3180 and 9455 {AA} J/A+AS/139/135 J/A+AS/139/135 The Optical Spectrum of RR Tel Line identifications and intensities for the optical spectrum of RR Telescopii between 3180 and 9455 {AA} F L Crawford F C McKenna F P Keenan L H Aller W A Feibelman S G Ryan Astron. Astrophys. Suppl. Ser. 139 135 1999 1999A&AS..139..135C Stars, variable Novae Spectroscopy binaries: symbiotic line: identifications stars: individual (RR Tel) The symbiotic nova RR Telescopii has been observed with the 3.9 m telescope at the Anglo-Australian Observatory (AAO), using the University College London Echelle Spectrograph (UCLES) in conjunction with a Tek CCD. It displays a rich emission line spectrum, ranging in excitation from NI to NiVIII. We present a list of 811 measured lines, with their suggested identifications and absolute line intensities, covering a wavelength range from 3180 to 9455 A. The absolute line intensities have been derived by comparing the high resolution data with a flux-calibrated low resolution spectrum taken with the Australian National University 2.3 m telescope. All of the lines have been successfully identified. Comparing our results with those of previous studies indicates that the RR Tel system is advancing towards higher degrees of ionisation.
RR Tel 20 00 20.2 -55 52 04
Line list for RR Telescopii, with absolute flux calibrated intensities shown, for the wavelength range 3490 - 5530{AA} Line list for RR Telescopii, in the wavelength range 3183 - 3488{AA} and 5550 - 9456{AA}, with intensities flux calibrated using the HeII recombination line ratios of Hummer & Storey (1987MNRAS.224..801H) and Storey & Hummer (1995MNRAS.272...41S) LambdaMea Measured wavelength 0.1nm DeltaV Velocity FWHM km/s n_DeltaV Note on DeltaV number=2 a: Measured intensities corrected for interstellar extinction using E(B-V)=0.08. b: Observed in the spectrum of a gaseous nebula (see McKenna et al., 1997ApJS..109..225M). c: Observed in the spectrum of eta Car (see McKenna et al., 1997ApJS..109..225M). d: In the case where more than one identification is listed for a given line, the first is taken to be the primary contributor to the blend. e: The estimated error in the line intensity is between 15 and 40%. k: The estimated error in the line intensity is between 20 and 40%. f: The estimated error in the line intensity is greater than 40%. g: It is possible that there may be some OVI at 3811.36 and 3834.24{AA}, but with the current data this is not definite. l: This HeII line is blended and so could not be used for calibration using line intensity ratios. h: There are several lines very close together here which could not be individually resolved, and so they are given as one line. i: These very wide features appear to be the Raman-scattered OVI lines at 6825 and 7082 {AA}, as shown by Espey et al. (1995ApJ...454L..61). --- Int Measured intensity 10-12mW/m2 Intc Corrected intensity number=1 Measured intensities corrected for interstellar extinction using E(B-V) = 0.08 (Jordan, Murset & Werner 1994A&A...283..475J) 10-12mW/m2 n_Intc Note on Intc number=2 a: Measured intensities corrected for interstellar extinction using E(B-V)=0.08. b: Observed in the spectrum of a gaseous nebula (see McKenna et al., 1997ApJS..109..225M). c: Observed in the spectrum of eta Car (see McKenna et al., 1997ApJS..109..225M). d: In the case where more than one identification is listed for a given line, the first is taken to be the primary contributor to the blend. e: The estimated error in the line intensity is between 15 and 40%. k: The estimated error in the line intensity is between 20 and 40%. f: The estimated error in the line intensity is greater than 40%. g: It is possible that there may be some OVI at 3811.36 and 3834.24{AA}, but with the current data this is not definite. l: This HeII line is blended and so could not be used for calibration using line intensity ratios. h: There are several lines very close together here which could not be individually resolved, and so they are given as one line. i: These very wide features appear to be the Raman-scattered OVI lines at 6825 and 7082 {AA}, as shown by Espey et al. (1995ApJ...454L..61). --- Line Identity of line --- n_Line Note on line number=3 j: The intrinsically stronger [NeV] line at 3426 is not detected, as it falls in a region between echelle orders. --- LambdaLab Laboratory wavelength 0.1nm n_LambdaLab Note on labLam number=2 a: Measured intensities corrected for interstellar extinction using E(B-V)=0.08. b: Observed in the spectrum of a gaseous nebula (see McKenna et al., 1997ApJS..109..225M). c: Observed in the spectrum of eta Car (see McKenna et al., 1997ApJS..109..225M). d: In the case where more than one identification is listed for a given line, the first is taken to be the primary contributor to the blend. e: The estimated error in the line intensity is between 15 and 40%. k: The estimated error in the line intensity is between 20 and 40%. f: The estimated error in the line intensity is greater than 40%. g: It is possible that there may be some OVI at 3811.36 and 3834.24{AA}, but with the current data this is not definite. l: This HeII line is blended and so could not be used for calibration using line intensity ratios. h: There are several lines very close together here which could not be individually resolved, and so they are given as one line. i: These very wide features appear to be the Raman-scattered OVI lines at 6825 and 7082 {AA}, as shown by Espey et al. (1995ApJ...454L..61). --- Mult Multiplet number --- F F: forbidden line --- Patricia Bauer CDS 1999 Jul 29 Fergal Crawford <Fergal.Crawford@Queens-Belfast.AC.UK> J_A+AS_139_135.xml The galaxy cluster Abell 426 (Perseus). A catalogue of 660 galaxy positions, isophotal magnitudes and morphological types J/A+AS/139/141 J/A+AS/139/141 Galaxies in the Perseus Cluster The galaxy cluster Abell 426 (Perseus). A catalogue of 660 galaxy positions, isophotal magnitudes and morphological types J Brunzendorf H Meusinger Astron. Astrophys. Suppl. Ser. 139 141 1999 1999A&AS..139..141B Clusters, galaxy Magnitudes Radial velocities Morphology galaxies: clusters: individual (A 426) galaxies: fundamental parameters galaxies: luminosity function A new catalogue of 660 galaxies within a field of about 10 square degrees in the Perseus cluster region is presented. The catalogue contains accurate positions, isophotal magnitudes, angular radii, position angles, radial velocities, morphological types, and detailed informations on morphological peculiarities. If available, cross identifications and radial velocities are also given. The catalogue is estimated to be complete to a 25mag isophotal B magnitude of about 18.
galaxies in A426 Sequence Running number in this catalogue --- Names Common names --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination (sign) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Mag25 Apparent B magnitude within B25 mag/arcsec^2^ isophote Without corrections for Galactic foreground extinction and inclination. mag u_Mag25 Uncertainty flag for Mag25 Typical uncertainties of Mag25 are 0.1 to 0.2 mag. Larger uncertainties due to difficulties in the removal of foreground stars are marked by a colon --- SuBr Central B surface brightness mag u_SuBr Uncertainty flag for SuBr --- a25 Major axis of the B25 mag/arcsec^2^ isophote arcsec b25 Minor axis of the B25 mag/arcsec^2^ isophote arcsec PA Position angle, North to East deg REM Remark number about size or photometry 1: a25, b25, PA are difficult to estimate for the individual components of this merger system 2: Mag25, a25, b25, PA are related to the central knot; the outer ring has a radius of 27 arcsec --- HRV Heliocentric radial velocity km/s Mtype Morphological Type --- n_Mtype Note on morphology and/or environment The following symbols are used: IN: systems with signs of strong interaction in the form of bridges (br) and/or tails (ta) DIS: systems with signs of distortions, which can show one or several of the following features coded by a number: (1) peculiar spiral arms (2) three-armed spirals (3) M51 type (4) unusual dust absorption (5) elliptical galaxy with isophote twist (6) non-concentric core (7) loops/shells (8) jet-like structures (9) fuzzy structure in the outer regions (10) radial spikes CH(n): n systems (n>1) within a common halo PL: polar ring galaxies or related objects f*: estimation of morphology hampered by a nearby foreground star The strength of the morphological peculiarity is indicated (+ for strong, - for weak). --- Helmut Meusinger TLS Tautenburg 1999 Jul 19 Helmut Meusinger <meus@obelix.tls-tautenburg.de> J_A+AS_139_141.xml HI observations of blue compact galaxies from the first and second Byurakan surveys. J/A+AS/139/1 J/A+AS/139/1 HI in Byurakan blue compact galaxies HI observations of blue compact galaxies from the first and second Byurakan surveys. T X Thuan V A Lipovetsky J -M Martin S A Pustilnik Astron. Astrophys. Suppl. Ser. 139 1 1999 1999A&AS..139....1T VII/172 : First Byurakan Survey (FBS) (Markarian+, 1989) Galaxies, radio H II regions H I data galaxies: compact galaxies: ISM galaxies: starburst radio lines: galaxies radio lines: ISM We present the results of a neutral hydrogen survey of 79 galaxies from a statistical sample of 88 Blue Compact Galaxies (BCGs) selected from the First and Second Byurakan objective prism surveys to have a HII region-like spectrum, an equivalent width of the [O III] {lambda}5007 line larger than ~50{AA}, and a velocity <=6000km/s. The detection rate for the statistical sample is 74%. HI masses range between 4x10^7^M_{sun}_ and 5x10^9^M_{sun}_ with the HI mass distribution peaking at 3x10^8^M_{sun}_. The full width at half-maximum of the HI profile varies between ~30km/s and 160km/s, with a mean of ~92km/s. These small widths are characteristic of dwarf galaxies. For comparison, we have also observed an additional 92 BCGs with weaker star formation and/or larger distances, and/or interesting astrophysical properties. These in general have larger widths and HI masses.
HI detections of BCGs Uncertain and confused HI detections BCG IAU name number=1 In table2.dat, UGC 6309 is not a BCG and has been observed to check for confusion with BCG 1114+517 = Mk 1445 In the original table, the name in the BCG column was "1114+5145" (SBS 1114+5145), and transformed in blanks here. --- m_Name Multiplictiy index on Name --- n_Name +: BCGs which are in the statistical sample *: galaxies non-confused in table2.dat a: See Note number=1 In table2.dat, UGC 6309 is not a BCG and has been observed to check for confusion with BCG 1114+517 = Mk 1445 In the original table, the name in the BCG column was "1114+5145" (SBS 1114+5145), and transformed in blanks here. --- Name Other name number=2 Mk: Markarian et al., 1989, Cat. <VII/172> UM: Michigan, Salzer et al., 1989ApJS...70..447S CG: Case, Pesh et al., 1991ApJS...76.1043P SB: Second Byurakan Survey, Markarian et al., 1983Afz....19...29M Stepanian et al., 1993BSAO...35...15S, 1993BSAO...35...24S 1993BSAO...35...32S, 1993BSAO...35...38S --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Dmaj Holmberg major diameter to the limiting surface brightness of B=26.5mag/arcsec^2^ arcsec --- --- Dmin Holmberg minor diameter to the limiting surface brightness of B=26.5mag/arcsec^2^ arcsec n_Dmaj Note on Size number=3 Size are mainly derived from CCD surface photometry (Lipovetsky et al., 1999, in prep.; Kniazev et al., 1995, priv. comm.). When CCD data was not available, Holmberg diameters were derived from measurements on the Palomar Sky Survey blue prints and the relation obtained by least-square fitting to the diameter data from a subsample of 48 of our BCGs with CCD photometry: d_H_(arcsec)=2.53d_PSS_(arcsec)+7.4". Diameters derived in this way are marked by the letter e. --- PA Position angle of the major axis of the galaxy measured eastward from north deg V(HI) Heliocentric HI velocity km/s e_V(HI) rms uncertainty on V(HI) km/s Dist Distance to the galaxy Mpc W50 Velocity width of the HI profile at 50% of the peak km/s e_W50 rms uncertainty on W50 km/s W20 Velocity width of the HI profile at 20% of the peak km/s e_W20 rms uncertainty on W20 km/s FluxObs Observed integrated flux density Jy.km/s e_FluxObs rms uncertainty on FluxObs Jy.km/s FluxCor HI flux density corrected for telescope beam size Jy.km/s e_FluxCor rms uncertainty on FluxCor Jy.km/s logM(HI) Hydrogen mass [solMass] Run Telescope used and year of observation number=4 Telescope used (G: Green Bank, N: Nancay) and the last two digits of the year of observation --- Note *: Note in notes.dat file --- HI non-detections of BCGs BCG IAU name --- m_Name Multiplictiy index on Name --- n_Name +: BCGs which are in the statistical sample --- Name Other name number=1 Mk: Markarian et al., 1989, Cat. <VII/172> UM: Michigan, Salzer et al., 1989ApJS...70..447S CG: Case, Pesh et al., 1991ApJS...76.1043P SB: Second Byurakan Survey, Markarian et al., 1983Afz....19...29M Stepanian et al., 1993BSAO...35...15S, 1993BSAO...35...24S 1993BSAO...35...32S, 1993BSAO...35...38S --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vopt Heliocentric optical velocity number=2 All optical velocities have been obtained with the 6m telescope IPCS with a typical accuracy of 100-150km/s. They come either from Stepanian et al., (1993BSAO...35...[15-38]S), or Lipovetsky et al.'s unpublished catalog of BCGs. km/s RMS rms noise of the spectrum mJy Run Telescope used and year of observation number=3 Telescope used (G: Green Bank, N: Nancay) and the last two digits of the year of observation --- Note *: Note in notes.dat file --- Indiviudal notes BCG IAU name --- m_BCG Multiplictiy index on BCG --- Note Text of the note --- Patricia Bauer CDS 1999 Oct 28 J_A+AS_139_1.xml New high proper motion stars with declinations between -5{deg} and -30{deg}, and right ascensions between 13h 30m and 24h J/A+AS/139/25 J/A+AS/139/25 New proper-motion stars -30<DE<-5, 13h30m<RA<24 New high proper motion stars with declinations between -5{deg} and -30{deg}, and right ascensions between 13h 30m and 24h H Wroblewski E Costa Astron. Astrophys. Suppl. Ser. 139 25 1999 1999A&AS..139...25W J/A+AS/78/231 : DE<-40, 0h<RA< 4h30m stars 1 to 144 (Wroblewski+ 1989) J/A+AS/91/129 : DE<-40, 4h30<RA<16h stars 145 to 521 (Wroblewski+ 1991) J/A+AS/105/179 : DE<-40, 16h<RA<24h stars 522 to 1069 (Wroblewski+ 1994) J/A+AS/115/481 : -30<DE<-5, 0h<RA<9h stars 1070 to 1563 (Wroblewski+ 1996) J/A+AS/122/447 : -30<DE<-5, 9h<RA<13h30m stars 1564 to 2055 (Wroblewski+ 1997) Proper motions astrometry stars: kinematics This table presents relative proper motions and positions for 293 stars with proper motions larger than 0.15 arcsec/year, discovered as a result of a program to identify fast moving stars in the southern hemisphere, being carried out with the Maksutov Astrograph at the Estacion astronomica de Cerro el Roble
Relative proper motions and positions of 293 newly discovered stars with proper motions larger than 0.15 arcsec/year WT List number --- Loc Location number number=1 The first two digits give the area number, and the remaining digits the star number. --- Bmag Blue photographic magnitude mag RAh Right ascension for J2000.0 h RAm Right ascension for J2000.0 min RAs Right ascension for J2000.0 s DE- Declination sign for J2000.0 --- DEd Declination for J2000.0 deg DEm Declination for J2000.0 arcmin DEs Declination for J2000.0 arcsec pm Total annual proper motion for J2000.0 arcsec/yr e_pm Total annual proper motion error arcsec/yr PA Position angle for J2000.0 deg Rem Remarks number=2 * identifies stars that are common to two overlapping areas. The implications of this are explained in Section 3 of the paper. --- Patricia Bauer CDS 1999 Jun 21 Edgardo Costa <costa@das.uchile.cl> J_A+AS_139_25.xml Empirical calibration of the lambda 4000 A break J/A+AS/139/29 J/A+AS/139/29 Empirical calibration of the 4000 A break Empirical calibration of the lambda 4000 A break J Gorgas N Cardiel S Pedraz J J Gonzalez Astron. Astrophys. Suppl. Ser. 139 29 1999 1999A&AS..139...29G J/ApJS/94/687 : Old stellar populations. V. (Worthey+, 1994) Stars, fundamental Effective temperatures Abundances, [Fe/H] stars: fundamental parameters galaxies: stellar content techniques: spectroscopic stars: atmospheres Empirical fitting functions, describing the behaviour of the {lambda}4000{AA} break in terms of effective temperature, metallicity and surface gravity, are presented. For this purpose, the break has been measured in 392 stars from the Lick/IDS Library. We have followed a very detailed error treatment in the reduction and fitting procedures, allowing for a reliable estimation of the break uncertainties. This calibration can be easily incorporated into stellar population models to provide accurate predictions of the break amplitude for, relatively old, composite systems. Table 1 lists the star sample, together with spectral types, adopted atmospheric parameters, break measurements, including errors, and residuals from the fitting functions.
Data sample and break measurements HD HD (Cat. <III/135>) name --- Name Alternative name --- SpType Spectral type number=1 Sources for spectral types are, in order of preference: Worthey et al. (1994, Cat. <J/ApJS/94/687>)), Gorgas et al. (1993ApJS...86..153G), the Bright Star Catalog (Hoffleit & Jaschek, 1982, Cat. <V/50>) and the SIMBAD database. For the cluster stars (except for Coma and Hyades) we list positions in the HR diagram (SGB: subgiant branch; GB: giant branch; HB: horizontal branch, red clump stars; AGB: asymptotic giant branch) --- Teff Effective temperature K r_Teff Source for effective temperature number=2 Atmospheric parameters are taken from the electronic table of Worthey et al (1994, Cat. <J/ApJS/94/687>), with the following additional sources and modifications: 1: Cayrel de Strobel et al. (1997A&AS..124..299C, Cat. <III/200>) 2: Alonso et al. (1996, Cat. <J/A+AS/117/227>) 3: Gratton et al. (1996, Cat. <J/A+A/314/191>) 4: Mean from sources 1, 2 and 3 5: Mean from sources 1 and 2 6: Mean from sources 1 and 3 7: Thevenin (1998BICDS.in.press.T) 8: Marsakov and Shevelev (1995BICDS..47...13M, Cat. <V/89>) 9: Gies and Lambert (1992ApJ...387..673G) 10: Zakhozhaj and Shaparenko (1996, Cat. <J/other/KFNT/12.20>) 11: Dyck et al. (1996AJ....111.1705D) 12: Computed from the indices Fe5270 and Fe5335 using the fitting functions of Gorgas et al. (1993ApJS...86..153G) (in terms of (V-K)) 13: Computed from the indices Fe5270 and Fe5335 using the fitting functions of Worthey et al. (1994, Cat. <J/ApJS/94/687>) (in terms of T_eff_) 14: Computed from the index Fe5270 using the fitting functions of Worthey et al. (1994, Cat. <J/ApJS/94/687>)) (in terms of T_eff_) 15: From spectral type using table III of Johnson (1966ARA&A...4..193J) 16: Extrapolation in the relation T_eff_ versus spectral type of Ridgway et al. (1980ApJ...235..126R) (these temperatures differ from those given by Worthey et al. (1994, Cat. <J/ApJS/94/687>)) --- log(g) Logarithm of gravity cm/s2 r_log(g) Source for logarithm of gravity number=2 Atmospheric parameters are taken from the electronic table of Worthey et al (1994, Cat. <J/ApJS/94/687>), with the following additional sources and modifications: 1: Cayrel de Strobel et al. (1997A&AS..124..299C, Cat. <III/200>) 2: Alonso et al. (1996, Cat. <J/A+AS/117/227>) 3: Gratton et al. (1996, Cat. <J/A+A/314/191>) 4: Mean from sources 1, 2 and 3 5: Mean from sources 1 and 2 6: Mean from sources 1 and 3 7: Thevenin (1998BICDS.in.press.T) 8: Marsakov and Shevelev (1995BICDS..47...13M, Cat. <V/89>) 9: Gies and Lambert (1992ApJ...387..673G) 10: Zakhozhaj and Shaparenko (1996, Cat. <J/other/KFNT/12.20>) 11: Dyck et al. (1996AJ....111.1705D) 12: Computed from the indices Fe5270 and Fe5335 using the fitting functions of Gorgas et al. (1993ApJS...86..153G) (in terms of (V-K)) 13: Computed from the indices Fe5270 and Fe5335 using the fitting functions of Worthey et al. (1994, Cat. <J/ApJS/94/687>) (in terms of T_eff_) 14: Computed from the index Fe5270 using the fitting functions of Worthey et al. (1994, Cat. <J/ApJS/94/687>)) (in terms of T_eff_) 15: From spectral type using table III of Johnson (1966ARA&A...4..193J) 16: Extrapolation in the relation T_eff_ versus spectral type of Ridgway et al. (1980ApJ...235..126R) (these temperatures differ from those given by Worthey et al. (1994, Cat. <J/ApJS/94/687>)) --- [Fe/H] Metallicity Sun r_[Fe/H] Source for metallicity number=2 Atmospheric parameters are taken from the electronic table of Worthey et al (1994, Cat. <J/ApJS/94/687>), with the following additional sources and modifications: 1: Cayrel de Strobel et al. (1997A&AS..124..299C, Cat. <III/200>) 2: Alonso et al. (1996, Cat. <J/A+AS/117/227>) 3: Gratton et al. (1996, Cat. <J/A+A/314/191>) 4: Mean from sources 1, 2 and 3 5: Mean from sources 1 and 2 6: Mean from sources 1 and 3 7: Thevenin (1998BICDS.in.press.T) 8: Marsakov and Shevelev (1995BICDS..47...13M, Cat. <V/89>) 9: Gies and Lambert (1992ApJ...387..673G) 10: Zakhozhaj and Shaparenko (1996, Cat. <J/other/KFNT/12.20>) 11: Dyck et al. (1996AJ....111.1705D) 12: Computed from the indices Fe5270 and Fe5335 using the fitting functions of Gorgas et al. (1993ApJS...86..153G) (in terms of (V-K)) 13: Computed from the indices Fe5270 and Fe5335 using the fitting functions of Worthey et al. (1994, Cat. <J/ApJS/94/687>) (in terms of T_eff_) 14: Computed from the index Fe5270 using the fitting functions of Worthey et al. (1994, Cat. <J/ApJS/94/687>)) (in terms of T_eff_) 15: From spectral type using table III of Johnson (1966ARA&A...4..193J) 16: Extrapolation in the relation T_eff_ versus spectral type of Ridgway et al. (1980ApJ...235..126R) (these temperatures differ from those given by Worthey et al. (1994, Cat. <J/ApJS/94/687>)) --- D4000 4000 A break --- e_D4000 Error on 4000 A break number=3 Total random errors in the lambda 4000 A break measurements --- Res Residual from the fitting functions number=4 Residuals from the derived fitting functions (observed minus predicted) --- Runs Runs in which the star was observed number=5 Run number(s) in which the star was observed. Number of repeated observations within each run is giving in parenthesis --- Comm Comments on individual stars number=6 Stars not used to derive the empirical functions are marked with: a: Non cluster members (see Gorgas et al., 1993ApJS...86..153G) b: Lacking required atmospheric parameters c: Emission-line supergiant --- Javier Gorgas UCM Patricia Bauer CDS 1999 May 18 Javier Gorgas <fjg@astrax.fis.ucm.es> J_A+AS_139_29.xml Photographic positions for the first eight satellites of Saturn J/A+AS/139/305 J/A+AS/139/305 Position of Saturn's satellites Photographic positions for the first eight satellites of Saturn C H Veiga R Vieira Martins Astron. Astrophys. Suppl. Ser. 139 305 1999 1999A&AS..139..305V J/A+AS/121/65 : 1990-1994 Saturn's satellites astrometry (Harper+ 1997) J/A+AS/136/257 : Saturn's satellites in 1995/97 (Harper+ 1999) J/A+AS/120/107 : 1989-1994 CCD observations of Triton (Veiga+ 1996) J/A+AS/131/291 : 1995-1997 CCD positions of Triton (Veiga+ 1998) J/A+AS/136/445 : CCD observations of Nereid (Veiga 1999) Planets Positional data astrometry planets and satellites: individual (Saturn) Astrometric positions of the first eight Saturnian satellites obtained from 138 photographic plates taken in 30 nights in the years 1982 to 1988 are presented. All positions are compared with those calculated by the theory TASS1.7 (Vienne & Duriez, 1998). The observed minus calculated residuals give rise to standard deviations smaller than 0.3".
*List of observed positions of the Saturnian satellite Opp Opposition year code number (105=1989, 111=1988) --- Obs.Y Year of observation yr Obs.M Month of observation --- Obs.D UTC date of observation (DD.dddddd) d ET-UTC ET-UTC to the nearest tenth of second s Code Observatory code (874: Laboratorio Nacional de Astrofisica) ---- Ref Reference code (no entries) --- ObsType Observation type ({Delta}RA, {Delta}DE) --- Sat Subject satellite, reference satellite number=1 Satellite numbers used in the catalogue conform to the conventional IAU numbering system. 0 is used to denote the planet. 1: Mimas; 2:Enceladus; 3: Tethys; 4: Dione; 5: Rhea; 6: Titan; 7: Hyperion; 8: Iapetus; 9: Phoebe --- Obs1 Presence flag for first observation of pair number=2 0: observation absent 1: observation present --- Obs2 Presence flag for second observation of pair number=2 0: observation absent 1: observation present --- DRA Position {Delta}RA s DDE Position {Delta}DE arcsec Sys Reference system (J2000.0) --- Frame Reference frame (geocentric) --- Res1 (O-C) {Delta}RAcosDE residual for first observation of pair arcsec Res2 (O-C) {Delta}RAcosDE residual for second observation of pair arcsec Patricia Bauer CDS 1999 Aug 05 Carlos Henrique Veiga <cave@obsn.on.br> J_A+AS_139_305.xml Multi-Frequency Study of the B3-VLA Sample. II. The database J/A+AS/139/359 J/A+AS/139/359 B3-VLA sample. II. The database Multi-Frequency Study of the B3-VLA Sample. II. The database M Vigotti L Gregorini U Klein K -H Mack Astron. Astrophys. Suppl. Ser. 139 1 1999 1999A&AS..139..359V VIII/37 : The Third Bologna Survey (B3) (Ficarra+ 1985) J/A+AS/133/129 : B3-VLA sample 10.6 GHz data (Gregorini+ 1998) Radio sources Spectroscopy radio continuum: general radio continuum: surveys Table 2 presents flux densities at 151, 327 and 408MHz and 1.4, 4.8 and 10.6GHz of B3-VLA sample and an updated list of the Optical Identifications of the sample.
B3-VLA flux densities B3 B3 name -- RAh Right Ascension (J2000) hours h RAm Right Ascension minutes min RAs Right Ascension seconds s DE- Declination sign --- DEd Declination (J2000) degree deg DEm Declination minutes arcmin DEs Declination seconds arcsec F151MHz Flux at 151 MHz number=1 At 151MHz 112 sources are missing, probably because they are fainter than the limiting flux density of the survey. Some fluxes are missing also at 408MHz due to blend of sources. At 10.6GHz there are some negative flux densities; their meaning is 3{sigma} Upper Limit. mJy e_F151MHz rms uncertainty on F151MHz mJy F327MHz Flux at 327 MHz number=1 At 151MHz 112 sources are missing, probably because they are fainter than the limiting flux density of the survey. Some fluxes are missing also at 408MHz due to blend of sources. At 10.6GHz there are some negative flux densities; their meaning is 3{sigma} Upper Limit. mJy e_F327MHz rms uncertainty on F327MHz mJy F408MHz Flux at 408 MHz number=1 At 151MHz 112 sources are missing, probably because they are fainter than the limiting flux density of the survey. Some fluxes are missing also at 408MHz due to blend of sources. At 10.6GHz there are some negative flux densities; their meaning is 3{sigma} Upper Limit. mJy e_F408MHz rms uncertainty on F408MHz mJy F1.4GHz Flux at 1.4 GHz mJy e_F1.4GHz rms uncertainty on F1.4GHz mJy F4.85GHz Flux at 4.85 GHz mJy e_F4.85GHz rms uncertainty on F4.85GHz mJy F10.6GHz Flux at 10.6 GHz mJy e_F10.6GHz rms uncertainty on F10.6GHz mJy ID Optical Identification number=2 Q: quasar b: blue object BL: BL Lac F: featureless spectrum g: galaxy with redshift < 0.5 G: galaxy with redshift > 0.5 blank: Empty Fields -- Patricia Bauer CDS 1999 Oct 07 Mario Vigotti <VIGOTTI@astbo1.bo.cnr.it> J_A+AS_139_359.xml Young massive star clusters in nearby galaxies. II. Software tools, data reductions and cluster sizes J/A+AS/139/393 J/A+AS/139/393 Young Massive Star Clusters. II. Young massive star clusters in nearby galaxies. II. Software tools, data reductions and cluster sizes S S Larsen Astron. Astrophys. Suppl. Ser. 139 393 1999 1999A&AS..139..393L Galaxies, nearby Associations, stellar Photometry, UBVRI photometry spiral star clusters techniques: image processing Table 4 lists photometric data for Young Massive Star Clusters identified in a sample of 21 nearby galaxies. The photometric data have been corrected for Galactic foreground extinction. Each cluster is identified by the abbreviated NGC number of its host galaxy and an object number: nxxx-yyy is object number yyy in the galaxy NGC xxx. Effective cluster radii have been obtained by modeling the cluster images as MOFFAT15 functions convolved with the point-spread function measured on the CCD images.
Photometric data for Young Massive Star Clusters ID Cluster identification (nxxx-yyy) --- xpos CCD X coordinate pix ypos CCD Y coordinate pix RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec VMAG Absolute Visual magnitude number=1 The distance moduli used for the absolute magnitudes and cluster sizes are listed in Larsen & Richtler, 1999A&A...345...59L (Paper I) mag U-B U-B colour index mag B-V B-V colour index mag V-I V-I colour index mag Reff Effective (half-light) radius pc Patricia Bauer CDS 1999 Jul 18 Soeren Larsen <soeren@astro.ku.dk> J_A+AS_139_393.xml CCD photometry and astrometry of visual double and multiple stars of the HIPPARCOS catalogue. II. CCD photometry and differential astrometry of 288 southern "intermediate" systems J/A+AS/139/425 J/A+AS/139/425 CCD Photometry and Astrometry of Double Stars CCD photometry and astrometry of visual double and multiple stars of the HIPPARCOS catalogue. II. CCD photometry and differential astrometry of 288 southern "intermediate" systems J Cuypers W Seggewiss Astron. Astrophys. Suppl. Ser. 139 425 1999 1999A&AS..139..425C I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Oblak et al., Paper I. 1999A&A...346..523O Stars, double and multiple Photometry, CCD stars: binaries: visual astrometry We present photometric and astrometric data of about 280 visual double stars of the "intermediate" class, i.e. with angular separations mainly in the range 2"<{rho}<12". The observations have been obtained in 1991-92 with a CCD camera attached to the 91cm Dutch telescope at ESO La Silla, Chile. Differential magnitudes of the double star components as well as magnitudes and colour indices of the individual components have been determined in the Cousins V and I passbands with an internal error of about 0.005mag and an external accuracy of less than 0.03mag. In addition, angular separations have been secured to an internal accuracy of 0.004" and position angles to about 0.05{deg}.
Hipparcos
Astrometric and photometric differential results (instrumental V and I) of the CCD observations for visual binaries Astrometric and photometric differential results (instrumental V and I) of the CCD observations for visual binaries with more than one sequence of measurements Name Star designation --- Note1 Standard type number=1 a: Astrometric standard p: Photometric standard --- Date Date of observation (Besselian year) yr Note2 Note to table1.dat number=2 *: more than one sequence of measurements (see Table 2) --- Nobs Total number of observations --- rho Mean separation arcsec e_rho Standard error of the mean separation arcsec theta Mean position angle deg e_theta Standard error of the mean position angle deg rVI Distance between the V and I parameters arcsec rNH Distance between this observation and the corresponding Hipparcos (Cat. <I/239>) result arcsec o_Vmag Number of observations in filter V --- DVmag Magnitude difference between component A and B in (instrumental) V mag e_DVmag Standard error of the mean magnitude difference between component A and B in (instrumental) V mag o_Imag Number of observations in filter I --- DImag Magnitude difference between component A and B in (instrumental) I mag e_DImag Standard error of the mean magnitude difference between component A and B in (instrumental) I mag Photometric results (V and I) of the CCD observations for visual binaries Photometric results (V and I) of the CCD observations for visual binaries with more than one sequence of measurements Name Star designation --- Note1 Strandard type number=1 a: Astrometric standard p: Photometric standard --- JD Julian date (2440000+) d Note2 Note to table3.dat number=2 *: more than one sequence of measurements (see Table 4) --- VmagA V magnitude of component A mag e_VmagA Standard error of the mean on V magnitude of component A mag VmagB V magnitude of component B mag e_VmagB Standard error of the mean on V magnitude of component B mag DVmag Magnitude difference between component A and B in V mag o_Vmag Number of observations in filter V --- V-IA Colour index V-I of component A mag e_V-IA Standard error of the mean of the colour index of component A mag V-IB Colour index V-I of component B mag e_V-IB Standard error of the mean of the colour index of component B mag o_Imag Number of observations in filter I --- DV-I Colour index V-I difference between component A and B mag Patricia Bauer CDS 1999 Sep 07 Jan Cuypers <Jan.Cuypers@oma.be> J_A+AS_139_425.xml Photometry and position observations of Saturnian satellites during their mutual eclipses and occultations in 1995 performed at the observatories in Russia and Kazakhstan J/A+AS/139/47 J/A+AS/139/47 1995 Saturnian satellites mutual events Photometry and position observations of Saturnian satellites during their mutual eclipses and occultations in 1995 performed at the observatories in Russia and Kazakhstan N V Emelianov T R Irsmambetova T P Kiseleva V G Tejfel S N Vashkovjak E A Glushkova V G Kornilov G A Charitonova Astron. Astrophys. Suppl. Ser. 139 47 1999 1999A&AS..139...47E J/AJ/103/983 : Stellar occultation candidates of Saturn (Bosh+, 1992) J/A+AS/121/65 : 1990-1994 Saturn's satellites astrometry (Harper+ 1997) J/A+AS/136/257 : Saturn's satellites in 1995/97 (Harper+ 1999) Planets Photometry Positional data Occultations astrometry occultation eclipses Satellites of Saturn The files contain the results of Photometry and Position Observations of Saturnian Satellites. Some file presents a specific data of each measurement. Common parameters of observations such as the initial moment are given in the article. Satelite number: --------------------- 1 Mimas 2 Enceladus 3 Tethys 4 Dione 5 Rhea 6 Titan 7 Hyperion 8 Iapetus ---------------------
*Photometry of mutual occultation (CL SAI) OBS.date Observation date "DD/MM/YY" OBS.h Observation date (hours) h --- --- OBS.m Observation date (minutes) min --- --- OBS.s Observation date (seconds) s Sat1 Number of the first satellite --- Sat2 Number of the second satellite --- Flux Measured flux (in relative units) --- *Photometry of mutual eclipse (FAI AS RK), OBS.DATE Observation date "DD/MM/YY" OBS.h hours of the moment (UTC) h OBS.m minute of the moment (UTC) min OBS.s seconds of the moment (UTC) s Sat1 Number of the first satellite --- Sat2 Number of the second satellite --- Flux Measured flux (in arbitrary units) --- *Mutual apparent angular distance measurements OBS.DATE Observation date "DD/MM/YY" Init.m Minutes from initial moment min Sat1 Number of the first satellite --- Sat2 Number of the second satellite or s for star --- Dist Apparent mutual distance arcsec CCD position observations (Pulkovo) OBS.DATE Date of observation "DD/MM/YY" OBS.h hours of the moment (UTC) h OBS.m minute of the moment (UTC) min OBS.s seconds of the moment (UTC) s Sat1 number of the first satellite --- Sat2 number of the second satellite --- Sep Angular distance between satellites arcsec PA Position angle for the first satellite deg e_Sep rms uncertainty on Sep arcsec e_PA rms uncertainty on PA deg Photographic observations (Pulkovo) OBS.Y year of observation yr OBS.M month of observation "month" OBS.D number with part of day (UTC) d Plate conditional number of photographic plate --- Sat1 Satellite number --- Sat2 Number of main body (0: planet, 6: Titan) --- xpos Coordinate x number=1 x=(RA1-RA2)cos(DE2), y=DE1-DE2, where RA1, DE1 is the position of the first satellite, Sat1 RA2, DE2 is the position of the second satellite, Sat2 arcsec ypos Coordinate y number=1 x=(RA1-RA2)cos(DE2), y=DE1-DE2, where RA1, DE1 is the position of the first satellite, Sat1 RA2, DE2 is the position of the second satellite, Sat2 arcsec e_xpos rms uncertainty on xpos arcsec e_ypos rms uncertainty on ypos arcsec Patricia Bauer CDS 1999 May 06 N. Emelianov <emelia@bdl.fr> J_A+AS_139_47.xml Kinematics of early-type galaxies in compact groups. HCG 67, HCG 74, and HCG 79 J/A+AS/139/483 J/A+AS/139/483 Early-type gal. kinematics in compact groups Kinematics of early-type galaxies in compact groups. HCG 67, HCG 74, and HCG 79 P Bonfanti F Simien R Rampazzo P Prugniel Astron. Astrophys. Suppl. Ser. 139 483 1999 1999A&AS..139..483B J/A+AS/122/521 : Kinematical data on early-type galaxies. I. (Simien+ 1997) J/A+AS/126/15 : Kinematical data on early-type galaxies. II. (Simien+ 1997) J/A+AS/126/519 : Kinematical data on early-type galaxies. III. (Simien+ 1997) J/A+AS/131/287 : Kinematical data on early-type galaxies. IV. (Simien+ 1998) Radial velocities Galaxies, rotation Velocity dispersion Clusters, galaxy galaxies: kinematics and dynamics galaxies: interactions galaxies: elliptical and lenticular, cD galaxies: formation galaxies: evolution We present measurements of stellar kinematics for seven early-type galaxies in HCG 67, HCG 74, and HCG 79. These data are aimed at studying the relation between the environment and the dynamics, structure and stellar content of early-type galaxies. In the present three groups, the kinematic features we observed cannot be associated unambiguously to physical interactions. Visible morphological peculiarities do not appear correlated with kinematical perturbations.
HCG 67a 13 49 11.3 -07 13 27.6 HCG 67d 13 49 09.7 -07 13 54.3 HCG 74a 15 19 24.7 +21 06 20.3 HCG 74b 15 19 24.4 +20 53 23.4 HCG 79a 15 59 11.4 +20 45 14.9 HCG 79b 15 59 12.6 +20 45 47.1 HCG 79c 15 59 10.9 +20 45 41.4
Main kinematical parameters from this study Name Object identification --- V0hel Heliocentric systemic velocity km/s e_V0hel Mean error on V0hel (rms) km/s sigma0 Projected central velocity dispersion km/s e_sigma0 Mean error on sigma0 km/s Profiles of rotation and velocity dispersion Name Object identification --- PA Position angle of slit number=1 Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0 of the component whose identification is given in bytes 1-9. deg r Radius (<0 and >0 on opposite semi-axes) number=1 Rotation and dispersion velocities are projected along the line of sight; rotation values are with respect to the point r=0 of the component whose identification is given in bytes 1-9. arcsec Vrot Proj. mean stellar rotation velocity number=2 For HCG67a, HCG79a, and HCG79b, PA has been shifted +180 degrees with respect to the printed version, in order to conform to the convention used by Simien & Prugniel (1997, Cat. <J/A+AS/126/519>), which is recalled below. PA (North --> East) is in the range [0, 360[, and: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s e_Vrot Mean error on Vrot km/s sigma Projected velocity dispersion number=2 For HCG67a, HCG79a, and HCG79b, PA has been shifted +180 degrees with respect to the printed version, in order to conform to the convention used by Simien & Prugniel (1997, Cat. <J/A+AS/126/519>), which is recalled below. PA (North --> East) is in the range [0, 360[, and: - for 0<PA<180, r<0 corresponds to the eastern side of the galaxy, - for 180<PA<360, r<0 corresponds to the western side, - and for PA=0, r<0 is to the North. km/s e_sigma Mean error on sigma km/s Patricia Bauer CDS 1999 Oct 19 Francois Simien <fs@cumulus.univ-lyon1.fr> J_A+AS_139_483.xml Multi-colour photometry of nearby dwarf galaxies J/A+AS/139/491 J/A+AS/139/491 BVI photometry of nearby galaxies Multi-colour photometry of nearby dwarf galaxies L Makarova Astron. Astrophys. Suppl. Ser. 139 491 1999 1999A&AS..139..491M Galaxies, nearby Photometry, CCD Photometry, Cousins galaxies: fundamental parameters galaxies: photometry galaxies: irregular galaxies: structure Integrated CCD-photometry of the dwarf nearby galaxies in B, V and I (Cousins) bands is presented. The photometry was performed in increasing circular apertures.
General parameters of the sample Name Galaxy name --- PGC PGC name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Type Galaxy type according to RC3 system --- D25 Angular diameter at the 25^m^ isophotal level arcmin Btot Total magnitude B_T_ mag AB Galactic absorption in B filter mag AV Galactic absorption in V filter mag AI Galactic absorption in I filter mag RV Radial velocity km/s Dist Galaxy distance Mpc Aperture photometry of the observed galaxies Name Galaxy name --- Rad Aperture radius arcsec Bmag Total B-magnitude within this aperture mag Vmag Total V-magnitude within this aperture mag Imag Total I-magnitude within this aperture mag Patricia Bauer CDS 1999 Aug 16 Sazonova Lida <lsaz@sao.ru> J_A+AS_139_491.xml Photometry of V1794 Cygni between 1975 and 1995 J/A+AS/139/513 J/A+AS/139/513 1975-1995 V1794 Cyg UBVRI photometry Photometry of V1794 Cygni between 1975 and 1995 L Jetsu I Tuominen B W Bopp O V Ezhkova K N Grankin T Hackman P A Heckert M A Ibragimov V B Kondratiev S Yu Mel'nikov T Oja H L Nations V S Shevchenko Astron. Astrophys. Suppl. Ser. 139 513 1999 1999A&AS..139..513J J/A+A/351/212 : V1794 UBVR time series (Jetsu+, 1999) Stars, variable Photometry, UBVRI stars: individual: (V1794 Cyg, HD 199178) variables techniques: photometric Six years of new photometry of V 1794 Cyg is combined with the previously published data. These data are processed into two decades of homogeneous standard Johnson UBVRI photometry, which contains 1207, 1837, 1927, 867 and 75 observations in U, B, V, R and I, respectively.
V1794 Cyg HD 199178 20 53 53.7 +44 23 11
The collected photometry of HD 199178 SET Subset number --- HJD Heliocentric Julian date d Umag U magnitude (0 = no observation) mag Bmag B magnitude (0 = no observation) mag Vmag V magnitude (0 = no observation) mag Rmag R magnitude (0 = no observation) mag Imag I magnitude (0 = no observation) mag Meas 0=normal measurement, 1=Flare, 2=Flare? --- table4.tex LaTeX version of table 4 Patricia Bauer CDS 1999 Sep 10 Lauri Jetsu <jetsu@gstar.astro.helsinki.fi> J_A+AS_139_513.xml A catalogue of velocities in the direction of the cluster of galaxies Abell 496 J/A+AS/139/525 J/A+AS/139/525 Abell 496 heliocentric velocities A catalogue of velocities in the direction of the cluster of galaxies Abell 496 F Durret P Felenbok C Lobo E Slezak Astron. Astrophys. Suppl. Ser. 139 525 1999 1999A&AS..139..525D VII/193 : The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995) J/A+AS/139/559 : A496 photometric catalogue (Slezak+, 1999) Clusters, galaxy Redshifts Photometry, CCD galaxies: clusters: individual (Abell 496) galaxies: clusters: general Catalogue of velocities for 466 galaxies in the direction of the cluster Abell 496, in a region covering about 160'x160' including previously published redshifts and redshifts from the CfA redshift survey.
Positions and magnitudes of stars StarNo Running number of star -- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign (2000.0) --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec bjmag bj magnitude mag Galaxy redshift catalogue GalNo Running number of galaxy -- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign (2000.0) --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec cz Heliocentric velocity km/s e_cz Error on heliocentric velocity km/s Rmag R magnitude mag Xpos X position relative to the X-ray centre number=1 Positions relative to the center assumed to have coordinates: RA = 04h 33m 37.9s, DE = -13{deg} 15' 47" (2000.0) arcsec Ypos Y position relative to the X-ray centre number=1 Positions relative to the center assumed to have coordinates: RA = 04h 33m 37.9s, DE = -13{deg} 15' 47" (2000.0) arcsec Dist Distance to the cluster centre arcsec TD Tonry & Davis (1979AJ.....84.1511T) parameter -- n_cz 0 = redshift from absorption lines, 1 = redshift from emission lines -- r_cz Label indicating redshift origin number=2 1: our data 2: Quintana & Ramirez, 1990AJ....100.1424Q 3: Malumuth et al., 1992AJ....104..495M 4: Proust et al., 1987A&AS...67...57P 5: Huchra et al., 1992, see Cat. <VII/193> -- Ref Cross-reference in various catalogues -- Patricia Bauer CDS 1999 Nov 12 Florence Durret <durret@iap.fr> J_A+AS_139_525.xml Survey of instantaneous 1-22 GHz spectra of 550 compact extragalactic objects with declinations from -30{deg} to +43{deg} J/A+AS/139/545 J/A+AS/139/545 1-22 GHz spectra survey Survey of instantaneous 1-22 GHz spectra of 550 compact extragalactic objects with declinations from -30{deg} to +43{deg} Y Y Kovalev N A Nizhelsky Yu A Kovalev A B Berlin G V Zhekanis M G Mingaliev A V Bogdantsov Astron. Astrophys. Suppl. Ser. 139 545 1999 1999A&AS..139..545K VIII/33 : Spectral characteristics of RATAN (RC) Catalog (Bursov+ 1989) VIII/49 : The Zelenchuk Surveys (Amirkhanyan+, 1989) J/A+AS/87/1 : RATAN-600 7.6 cm catalog of radio sources (Parijskij+ 1991) J/AZh/62/229 : Giant H II region Ratan-600 observations (Berlin+ 1985) J/AZh/74/42 : RATAN-600 radio sources spectra (Bursov 1997) J/other/BSAO/40.128 : RATAN-600 radio sources spectra (Bursov 1996) J/other/BSAO/40.5 : RATAN-600 RC radio sources (Parijskij+ 1996) Radio sources Radio lines Redshifts galaxies: active galaxies: compact BL Lacertae objects: general quasars: general radio continuum: galaxies radio continuum: general We present observational results for extragalactic radio sources with milliarcsecond components, obtained with the 600 meter ring radio telescope RATAN-600 from 1st to 22nd December, 1997. For each source, a six frequency broad band radio spectrum was obtained by observing simultaneously with an accuracy up to a minute at 1.4, 2.7, 3.9, 7.7, 13 and 31 cm. The observed list is selected from Preston et al. (1985AJ.....90.1599P) VLBI survey and contains all the sources in the declinations between -30 and +43 degrees with a correlated flux density exceeding 0.1 Jy at 13 cm. The sample includes the majority of sources to be studied in the current VSOP survey and the future RadioAstron Space VLBI mission.
Sources sample IAU IAU name (based on 1950 positions) --- Name Other name when available --- RAh Right ascension (B1950) number=1 B1950 coordinates are taken from Preston et al. (1985AJ.....90.1599P) and Morabito et al. (1986AJ.....91.1038M). h RAm Right ascension (B1950) number=1 B1950 coordinates are taken from Preston et al. (1985AJ.....90.1599P) and Morabito et al. (1986AJ.....91.1038M). min RAs Right ascension (B1950) number=1 B1950 coordinates are taken from Preston et al. (1985AJ.....90.1599P) and Morabito et al. (1986AJ.....91.1038M). s DE- Declination sign (B1950) number=1 B1950 coordinates are taken from Preston et al. (1985AJ.....90.1599P) and Morabito et al. (1986AJ.....91.1038M). --- DEd Declination (B1950) number=1 B1950 coordinates are taken from Preston et al. (1985AJ.....90.1599P) and Morabito et al. (1986AJ.....91.1038M). deg DEm Declination (B1950) number=1 B1950 coordinates are taken from Preston et al. (1985AJ.....90.1599P) and Morabito et al. (1986AJ.....91.1038M). arcmin DEs Declination (B1950) number=1 B1950 coordinates are taken from Preston et al. (1985AJ.....90.1599P) and Morabito et al. (1986AJ.....91.1038M). arcsec OI Optical identification number=2 Optical identifications (OI) andred shifts are taken from Veron-Cetty & Veron (1998, Cat. <VII/207>) or, if not found there, are taken from the NASA/IPAC Extragalactic database (NED). The abbreviations used are "Q" for quasars, "BL" for BL Lacertae objects, "G" for galaxies, "RS" for radio sources. In the latter case we do not have OI. --- Sp Spectrum classification number=3 Optical spectrum classification is taken from Veron-Cetty & Veron (1998, Cat. <VII/207>). --- l_z limit on z number=2 Optical identifications (OI) andred shifts are taken from Veron-Cetty & Veron (1998, Cat. <VII/207>) or, if not found there, are taken from the NASA/IPAC Extragalactic database (NED). The abbreviations used are "Q" for quasars, "BL" for BL Lacertae objects, "G" for galaxies, "RS" for radio sources. In the latter case we do not have OI. --- z Redshift number=2 Optical identifications (OI) andred shifts are taken from Veron-Cetty & Veron (1998, Cat. <VII/207>) or, if not found there, are taken from the NASA/IPAC Extragalactic database (NED). The abbreviations used are "Q" for quasars, "BL" for BL Lacertae objects, "G" for galaxies, "RS" for radio sources. In the latter case we do not have OI. --- Fc Correlated flux density at 13 cm number=4 Correlated flux density at 13 cm with errors are taken from Preston et al. (1985AJ.....90.1599P). Jy e_Fc Error on the correlated flux density number=4 Correlated flux density at 13 cm with errors are taken from Preston et al. (1985AJ.....90.1599P). Jy 1-22 GHz instantaneously measured broad band spectra data IAU IAU name (based on 1950 positions) --- F1.4cm Flux density at 1.4 cm Jy e_F1.4cm Error on the flux density at 1.4 cm Jy F2.7cm Flux density at 2.7 cm Jy e_F2.7cm Error on the flux density at 2.7 cm Jy F3.9cm Flux density at 3.9 cm Jy e_F3.9cm Error on the flux density at 3.9 cm Jy F7.7cm Flux density at 7.7 cm Jy e_F7.7cm Error on the flux density at 7.7 cm Jy F13cm Flux density at 13 cm Jy e_F13cm Error on the flux density at 13 cm Jy F31cm Flux density at 31 cm Jy e_F31cm Error on the flux density at 31 cm Jy Yuri Y. Kovalev ASC 1999 Aug 24 Yuri Kovalev <yyk@dpc.asc.rssi.ru> J_A+AS_139_545.xml A photometric catalogue of galaxies in the cluster Abell 496. J/A+AS/139/559 J/A+AS/139/559 Abell 496 photometric catalogue A photometric catalogue of galaxies in the cluster Abell 496. E Slezak F Durret J Guibert C Lobo Astron. Astrophys. Suppl. Ser. 139 559 1999 1999A&AS..139..559S J/A+AS/139/525 : Abell 496 heliocentric velocities (Durret+ 1999) Clusters, galaxy Magnitudes galaxies: clusters: individual (Abell 496) galaxies: clusters: general Two catalogues of galaxies in the direction of the cluster Abell 496 are presented. The first one includes 3,879 galaxies located in a region roughly +/-1.3 degree from the cluster centre ; it has been obtained by scanning part of a Schmidt photographic plate taken in the Bj band. Positions are very accurate but magnitudes are not. A second catalogue gives a list of galaxies with CCD magnitudes in the V (239 galaxies) and R (610 galaxies) bands for a much smaller region in the centre of the cluster.
Galaxy candidates from the SRC-J 621 plate Seq1 Running number -- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign (2000.0) --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec amaj Half major axis arcsec e Eccentricity -- PA Position angle of the major axis deg bjmag bj magnitude mag Xpos X position relative to the X-ray centre number=1 Coordinates of the X-ray centre: RA = 04h 33m 37.9s, DE= -13{deg} 15' 47" (2000.0) arcsec Ypos Y position relative to the X-ray centre number=1 Coordinates of the X-ray centre: RA = 04h 33m 37.9s, DE= -13{deg} 15' 47" (2000.0) arcsec Dist Distance to the cluster centre arcsec MAMA MAMA catalogue reference number -- Seq2 Number in table2 --- Galaxy candidates from CCD imaging Seq2 Running number -- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign (2000.0) --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec e Eccentricity -- PA Position angle of the major axis (from North to East) deg Vmag V magnitude mag Rmag R magnitude mag Xpos X position relative to the X-ray centre number=1 Coordinates of the X-ray centre: RA = 04h 33m 37.9s, DE= -13{deg} 15' 47" (2000.0) arcsec Ypos Y position relative to the X-ray centre number=1 Coordinates of the X-ray centre: RA = 04h 33m 37.9s, DE= -13{deg} 15' 47" (2000.0) arcsec Dist Distance to the cluster centre arcsec Seq1 Number in Table 1 -- Patricia Bauer CDS 1999 Nov 12 Florence Durret <durret@iap.fr> J_A+AS_139_559.xml UBV absolute CCD photometry and differential astrometry of a sample of visual double stars with A-type primaries J/A+AS/139/69 J/A+AS/139/69 UBV Astrometry and Photometry of doubles UBV absolute CCD photometry and differential astrometry of a sample of visual double stars with A-type primaries N Shatsky D Sinachopoulos P Prado E van Dessel Astron. Astrophys. Suppl. Ser. 139 69 1999 1999A&AS..139...69S I/237 : The Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996) Stars, double and multiple Photometry, UBV stars: binaries: visual techniques: photometric astrometry UBV CCD absolute photometry and differential astrometry of 111 southern visual binaries are presented. Observations have been performed at Las Campanas Observatory (Chile) in 1991-92 at 61-cm telescope. The separation range is 2.5-8arcsec. The mean epoch of the measurements is 1992.0. The photometry (table 1) was calibrated by one night of standard star observations. The positional parameters (table 3) are given in the reference system J2000 and calibrated using Hipparcos and CDS data. An additional table 2 provides the notes on observational circumstances.
Photometric data RAh Right ascension: hours (J2000) number=1 Taken from "The Washington Visual Double Star Catalog", US Naval Observatory (Worley C.E., Douglass G.G., 1996, Cat. <I/237>) h RAdm Right ascension: deci-minutes (J2000) 0.1min DE- Declination sign --- DEd Declination: degrees (J2000) deg DEm Declination: minutes (J2000) arcmin DM Durchmusterung designation number=2 Corresponds to the particular durchmusterung depending on declination: Zone = [+89,-22]: Bonn Durchmusterung Zone = [-23,-51]: Cordoba Durchmusterung Zone = [-52,-89]: Cape Durchmusterung --- Comp Component designation number=1 Taken from "The Washington Visual Double Star Catalog", US Naval Observatory (Worley C.E., Douglass G.G., 1996, Cat. <I/237>) --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag number=3 For secondaries (Comp="B") this error is that of differency of magnitude or colour, measured between the secondary and primary components. mag U-B Colour index mag e_U-B rms uncertainty on U-B number=3 For secondaries (Comp="B") this error is that of differency of magnitude or colour, measured between the secondary and primary components. mag B-V Colour index mag e_B-V rms uncertainty on B-V number=3 For secondaries (Comp="B") this error is that of differency of magnitude or colour, measured between the secondary and primary components. mag Nobs Number of observations --- Note Note in table 2 --- Notes RAh Right ascension: hours (J2000) number=1 Taken from "The Washington Visual Double Star Catalog", US Naval Observatory (Worley C.E., Douglass G.G., 1996) h RAdm Right ascension: decimals of minutes (J2000) 0.1min DE- Declination sign --- DEd Declination: degrees (J2000) deg DEm Declination: minutes (J2000) arcmin Note Note for object observations --- Positional parameters RAh Right ascension: hours (J2000) h RAdm Right ascension: decimals of minutes (J2000) 0.1min DE- Declination sign --- DEd Declination: degrees (J2000) deg DEm Declination: minutes (J2000) arcmin HIP Hipparcos Output Catalogue (Cat. <I/239>) number --- rho Separation arcsec e_rho rms uncertainty on rho number=1 includes calibration uncertainties arcsec theta Positional angle (J2000) deg e_theta rms uncertainty on theta number=1 includes calibration uncertainties deg Nobs Number of observations --- Patricia Bauer CDS 1999 Jun 04 Nicolaj Ivanovich Shatsky <kolja@sai.msu.ru> J_A+AS_139_69.xml HI properties of nearby galaxies from a volume-limited sample J/A+AS/139/97 J/A+AS/139/97 HI properties of nearby galaxies HI properties of nearby galaxies from a volume-limited sample I D Karachentsev D I Makarov W K Huchtmeier Astron. Astrophys. Suppl. Ser. 139 97 1999 1999A&AS..139...97K Galaxies, nearby H I data galaxies: global HI parameters galaxies The Appendix contains 318 galaxies, 15 of them with Vo>500km/s but D<10Mpc, and 28 dwarf spheroidals without Vo but highly probable members of nearby groups.
Parameters of nearby galaxies Name Galaxy designation --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min DE- Declination sign (1950.0) --- DEd Declination (1950.0) deg Btot Total magnitude in B band mag RV Corrected radial velocity (KM86) number=2 KM86: Karachentsev I.D., Makarov D.I., 1996AJ....111..794K km/s Mtype Morphological type code --- Dist Distance Mpc Dtype Note on distance number=1 P: photometric M: membership H: Hubble law --- Tidal Tidal index --- logDiam log(corrected linear diameter) [kpc] logL log(L/L_{sun}_) [solLum] logVm log(rotational velocity) [km/s] logM25/L log(M(25)/L) [Sun] logMHI/L log(M(HI)/L) [Sun] logMHI/M25 log(M(HI)/M(25)) -- muB Optical surface brightness mag/arcsec2 Patricia Bauer CDS 1999 Sep 13 Dmitry Makarov <dim@sao.ru> J_A+AS_139_97.xml Period-luminosity-colour distribution and classification of galactic oxygen-rich LPVs. I. Luminosity calibrations. J/A+AS/140/55 J/A+AS/140/55 Pulsation of galactic long-period variables Period-luminosity-colour distribution and classification of galactic oxygen-rich LPVs. I. Luminosity calibrations. D Barthes X Luri R Alvarez M O Mennessier Astron. Astrophys. Suppl. Ser. 140 55 1999 1999A&AS..140...55B I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) II/214 : Combined General Catalogue of Variable Stars (Kholopov+ 1998) Stars, variable stars: variables: long-period variables AGB fundamental parameters kinematics evolution The absolute K magnitudes and kinematic parameters of about 350 oxygen-rich Long-Period Variable stars are calibrated, by means of an up-to-date maximum-likelihood method, using Hipparcos parallaxes and proper motions together with radial velocities and, as additional data, periods and V-K colour indices. Four groups, differing by their kinematics and mean magnitudes, are found. For each of them, we also obtain the distributions of magnitude, period and de-reddened colour of the base population, as well as de-biased period-luminosity-colour relations and their two-dimensional projections. The SRa semiregulars do not seem to constitute a separate class of LPVs. The SRb appear to belong to two populations of different ages. In a PL diagram, they constitute two evolutionary sequences towards the Mira stage. The Miras of the disk appear to pulsate on a lower-order mode. The slopes of their de-biased PL and PC relations are found to be very different from the ones of the Oxygen Miras of the LMC. This suggests that a significant number of so-called Miras of the LMC are misclassified. This also suggests that the Miras of the LMC do not constitute a homogeneous group, but include a significant proportion of metal-deficient stars, suggesting a relatively smooth star formation history. As a consequence, one may not trivially transpose the LMC period-luminosity relation from one galaxy to the other.
List of the sample stars HIP Hipparcos <Cat. <I/239>) code number --- Name GCVS (Cat. <II/214>) name --- Type Variability type --- Period Pulsation period d Rem Remarks: radial velocity or J mag unavailable --- Patricia Bauer CDS 1999 Sep 10 Dominique Barthes <barthes@pchpc4.am.ub.es> J_A+AS_140_55.xml Determination of the radii of Cepheids. V. Radial velocities and dimensions of 22 galactic Cepheids J/A+AS/140/79 J/A+AS/140/79 Radii of 22 galactic Cepheids Determination of the radii of Cepheids. V. Radial velocities and dimensions of 22 galactic Cepheids M Imbert Astron. Astrophys. Suppl. Ser. 140 79 1999 1999A&AS..140...79I Stars, variable Radial velocities stars: Cepheids stars: fundamental parameters techniques: radial velocities We present radial velocity data for 22 galactic Cepheid stars obtained with Coravel spectrometer. Continuous observation over several years has enabled us to obtain 852 individual velocities covering all the phases of the pulsation. The mean number of measurements per star is 39, ranging from 20 to 113. For each star radial velocity versus phase diagrams have been fitted by analytical relation, and the stellar radius variation has been derived by integration of this relation over the whole period. Using recent ubv photometry of the literature and velocity curves, we have calculated the radii of the stars using a method based on the Baade-Wesselink concept. For these 22 Cepheids we give a linear logarithmic period-radius relation with a range of 2,4 to 45 days.
Star positions (from Simbad database) Name Star name --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Observed radial velocities, O-C and phases Name Star name --- OBS.date UT date of observation (dd/mm/yy) "DD/MM/YY" OBS.h UT date of observation (hh) h --- --- OBS.m UT date of observation (mm) min HJD Heliocentric Julian date d RV Observed radial velocity km/s O-C Observed - calculated radial velocity km/s Phase Phase --- e_RV Standard error of RV km/s table1.tex LaTeX version of table1 Patricia Bauer CDS 1999 Sep 14 M. Imbert <maurice.imbert@observatoire.cnrs-mrs.fr> J_A+AS_140_79.xml Line Blocking and equivalent widths in the spectrum of Pollux J/A+AS/42/391 J/A+AS/42/391 Line Blocking and equivalent widths in the spectrum Line Blocking and equivalent widths in the spectrum of Pollux F Ruland R Griffin R Griffin D Biehl H Holweger Astron. Astrophys. Suppl. Ser. 42 391 1980 1980A&AS...42..391R spectroscopy stars: late-type High-dispersion spectrograms of Pollux (beta Gem, K0III) have been used to derive line blocking coeffecients for the spectral range 4900-9300 A, and equivalent widths of lines of 43 atoms, ions, and molecules.
Equivalent widths of atomic and ionic lines measured from the spectrum of Pollux. Lambda Wavelength in Angstroem 0.1nm Ion Ion designation --- Mult Multiplet number --- W Equivalent width of line in Pollux in milliAngstroem 0.1pm Equivalent widths of molecular lines in Pollux Lambda Wavelength in Angstroem 0.1nm Mol Molecule designation --- W Equivalent width of line in Pollux in milliAngstroem 0.1pm M.J. Wagner, Francois Ochsenbein CDS 1993 Jul 27 J_A+AS_42_391.xml The gas distribution in the central region of the Galaxy. IV. A survey of neutral hydrogen in the region 349 < l < 13, -10 < b < 10, |v| < 350 km/s J/A+AS/52/63 J/A+AS/52/63 H I Survey of the Galactic Center Region The gas distribution in the central region of the Galaxy. IV. A survey of neutral hydrogen in the region 349 < l < 13, -10 < b < 10, |v| < 350 km/s W B Burton H S Liszt Astron. Astrophys. Suppl. Ser. 52 63 1983 1983A&AS...52..63B H I data Interstellar matter Surveys Radio sources Galaxy: structure ISM: clouds ISM: general ISM: kinematics and dynamics surveys Presented here are 21-cm observations of neutral hydrogen emission from the core of our Galaxy made over a period of several years with the 140-foot telescope of the National Radio Astronomy Observatory. The survey covers the region 348 < l < 10, -10 < b < 10 with an angular resolution of 21' and a grid spacing of 0.5 degrees in both l and b, and the velocity range |v| < 310 km/s with a kinematic resolution of 5.5 km/s. The sensitivity of the data generally corresponds to an antenna-temperature rms level of 0.02 K or better. The H I spectra from the survey are archived in a single three-dimensional (v, l, b) data cube in FITS image format. There are 224 velocity channels with a step of 2.75 km/s between channels. The intensities are given in units of antenna temperature and can be converted to brightness temperature units by multiplying by a factor of (1.52).
hicenter.fit velocity-longitude-latitude data cube for entire survey T. Sodroski ADF/ADC 1999 Nov 30 We thank the authors for making the data available for public distribution. J_A+AS_52_63.xml Magnitudes, colors and positions for bright stars in the Large Magellanic Cloud bar J/A+AS/61/473 J/A+AS/61/473 BV photometry in the LMC bar Magnitudes, colors and positions for bright stars in the Large Magellanic Cloud bar M Bernazzani R Buonanno C E Corsi E Hardy Astron. Astrophys. Suppl. Ser. 61 473 1985 1985A&AS...61..473B Magellanic Clouds Photometry Magellanic Clouds photometry We present B, V magnitudes and relative positions for all brighter than V=18.3 in a field of 0.02 square degrees near the north west end of the Large Magellanic Cloud bar. These star are the bright tail of a larger sample of about 18000 stars previously presented in the form color-magnitude diagram; they form a set of data free from selection effects and, therefore, valuable for further studies.
Magnitudes, colors and positions for the stars in HEA (1984ApJ...278..592H) ID Star identification --- Vmag V magnitude mag B-V B-V color index mag Xpos X position number=1 X coordinate increases from North to South, Y from Weast to East. arcsec Ypos Y position number=1 X coordinate increases from North to South, Y from Weast to East. arcsec Patricia Bauer CDS 1996 Sep 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_61_473.xml On the relation of Markarian galaxies with Zwicky clusters. I. Data J/A+AS/65/349 J/A+AS/65/349 Markarian galaxies and Zwicky clusters relations On the relation of Markarian galaxies with Zwicky clusters. I. Data A R Petrosian M Turatto Astron. Astrophys. Suppl. Ser. 65 349 1986 1986A&AS...65..349P VII/172 : First Byurakan Survey (FBS) (Markarian+, 1989) I/49 : Galaxies and Clusters of Galaxies (CGCG) (Zwicky, 1968) Petrosian & Turatto, Paper II. Discussion =1986A&A...163...26P Clusters, galaxy Galaxies, Markarian galaxies: clusters: general galaxies: Markarian In the same area covered by Markarian survey and CGCG, there are 1344 Markarian galaxies, of which 597 are positioned inside the contours of Zwicky clusters. Data on these galaxies and respective clusters are presented in different tables, according to whether they are galaxies which are members of clusters, or probable or possible members projection cases are considered separately.
Markarian galaxies which are real members of the Zwicky clusters with only one redshift value determined with more than one galaxy (counting Markarian galaxies) Cluster Cluster designation by right ascension and declination (1950) --- n_Cluster Note on Cluster --- Type Cluster type --- HRVc Cluster heliocentric radial velocity km/s n_HRVc Note on HRVc number=1 ': Cluster velocities recalculated with velocities of Markarian galaxies which are new members of clusters --- NGal Number of galaxies with published redshifts used to compute the mean HRV --- Mrk Markarian galaxy designation (see Cat. <VII/172>) --- HRVm Markarian galaxy heliocentric radial velocity km/s r_HRVm References of the Markarian galaxy velocity (See ref file) --- Note * : individual note number=2 Zw 0310.0-0130: Two background objects with V=9200km/s from B-PPV were used for calculation of cluster mean velocity. Zw 0801.3+3954: Background object with V=10020km/s from B-PPV was used for calculation of cluster mean velocity. Zw 0819.6+2209: Markarian galaxies are members of <D> and <A> subgroups of Bothun et al. (1983ApJ...268...47B) respectively. Zw 0837.0+2506: The galaxy with V=5420km/s is B-PPV is NGC 2623. Its diameter is about three times that of real members of the cluster It is probably a foreground object. Zw 1051.4+4041: Cluster velocity taken similar to Shahbazian 1 (Kirshner and Malumuth, 1980ApJ...236..366K). Zw 1144.0+5555: Mrk 1455 is also a member of the background group of Zw 1138.7+5650. --- Notes Notes number=3 Geller-Huchra groups (GH) of galaxies, (Geller & Huchra, 1983, Cat. <VII/84>), Abell clusters, Abell (1958, Cat. <VII/4>), coincident with Zwicky clusters or other clusters denominations are given --- Cases in which clusters have two or more values of mean velocity in B-PPV (Baieisi-Pillastrini et al., 1984A&AS...56..363B) and their differences are more the 200km/s. Markarian galaxies is a member of one subgroup Cluster Cluster and subgroup designation by right ascension and declination (1950) --- m_Cluster Multiplicity index on Cluster --- Type Cluster type --- HRVc Heliocentric radial velocity from B-PPV of each subgroup in the cluster. km/s n_HRVc Note on HRVc number=1 ': Subgroup velocities recalculated with velocities of Markarian galaxies which are new members of the subgroup --- NGal Number of galaxies with published redshifts used to compute the mean HRV --- Mrk Markarian galaxy designation (see Cat. <VII/172>) --- HRVm Markarian galaxy heliocentric radial velocity km/s r_HRVm [1/14] References of the Markarian galaxy velocity (See ref file) --- Note *: individual notes number=2 Zw 0826.2+3039: The diameter of Mrk 390 is 0.40mm and the mean diameter for cluster galaxies is 0.37+/-0.13mm. Zw 0926.5+3026: Mrk 401 with five other neighbours have diameters of 1.00mm and the mean diameter for other cluster members is 0.36+/-0.11mm. Zw 0957.9+1111: There are two systems of diameters, d1=0.44+/-0.12mm and d2=1.00+/-0.10mm, in the cluster. <A> subgroup velocity with IC 584 (d=1.00mm); <B> subgroup introduced by us with velocity from Mrk 1241 (d=0.30mm). Zw 1655.8+6844: Mrk 1110 is probably a member of V 107 ({DELTA}V=2200km/s). Zw 1707.6+4045: The diameter of Mrk 501 is 0.80mm and the mean diameter for cluster galaxies is 0.65+/-0.13mm. The galaxy with V=2110km/s is NGC 6339 (d=2.55mm). It is probably a foreground object. --- Notes Notes number=3 GH (Geller & Huchra, 1983, Cat. <VII/84>) and V (Vennik, 1984, A List of Nearby Groups of Galaxies, Tallin, USSR) groups, Abell clusters, Abell (1958, Cat. <VII/4>), coincident with subgroups of Zwicky clusters are given --- Cases of Markarian galaxies which are members of foreground or background groups containing more than one galaxy. All these groups are from the notes of B-PPV Cluster Designation by right ascension and declination (1950) of cluster and subgroups having foreground or background groups --- m_Cluster Multiplicity index on Cluster --- HRVc Heliocentric radial velocity of the cluster or the the subgroups km/s n_HRVc Note on HRVc number=1 ': Subgroup velocities recalculated with velocities of Markarian galaxies which are new members of clusters Other velocities are from B-PPV --- NGal Number of galaxies used to compute the mean HRV --- HRVg Group heliocentric radial velocity km/s n_HRVg Note on HRVg number=2 ': Group velocities recalculated with velocities of Markarian galaxies which are members of this group --- NGal2 Number of galaxies with published redshifts used to compute the mean HRV --- Mrk Markarian galaxy designation (see Cat. <VII/172>) --- HRVm Markarian galaxy heliocentric radial velocity km/s r_HRVm [1/14] References of the Markarian galaxy velocity (See ref file) --- Note * : individual notes number=3 Zw 1138.7+5650: Galaxies Mrk 184, 1456 and 1457 have velocities similar to the cluster Zw 1144.0+5555 but they are located out of its contour. Mrk 1455 is a member of both clusters. Zw 1424.0+2613: Mrk 673 is a member of the cluster Zw 1424+2613B (Noonane, 1981ApJS...45..613N). Zw 1600.4+1925: See Chincarini and Martins (1975ApJ...196..335C). --- Notes Notes number=4 GH (Geller & Huchra, 1983, Cat. <VII/84>) and V (Vennik, 1984, A List of Nearby Groups of Galaxies, Tallin, USSR) groups coincident with foreground or background groups. Other cluster denominations are given --- Cases in which Markarian galaxy is the only object with measured redshift in the cluster Cluster Cluster designation by right ascension and declination (1950) --- Dist Cluster distance class --- Type Cluster type --- Mrk Markarian galaxy designation (see Cat. <VII/172>) --- HRVm Markarian galaxy heliocentric radial velocity km/s r_HRVm References of the Markarian galaxy velocity (See ref file) --- Diam Markarian galaxy diameter mm Diam10 Mean value of diameters of 10 near galaxies mm e_Diam10 rms uncertainty on Diam10 mm Note * : individual notes number=1 Zw 0921.6+2354: Projection is possible (see B-PPV and Turatto and Petrosian, 1985ATsir1371....1T). Zw 1224.6+3131: The galaxy with V=725km/s in B-PPV is NGC 4414 (d~4.0mm and mp=10.9). It is probably a foreground object. --- Notes Notes --- Markarian galaxies which are probable members of clusters (2000km/s<{DELTA}V<4000km/s) Cluster Cluster designation by right ascension and declination (1950) --- m_Cluster Multiplicity index on Cluster --- Type Cluster type --- HRVc Cluster heliocentric radial velocity km/s n_HRVc Note on HRVc number=1 ': Cluster velocities recalculated with velocities of Markarian galaxies which are new members of clusters --- NGal Number of galaxies with published redshifts used to compute the mean HRV --- Mrk Markarian galaxy designation (see Cat. <VII/172>) --- HRVm Markarian galaxy heliocentric radial velocity km/s r_HRVm [1/14] References of the Markarian galaxy velocity (See ref file) --- Notes Notes --- Markarian galaxies which are projected on the cluster (V>4000km/s) Cluster Cluster designation by right ascension and declination (1950) (See Zwicky CGCG <I/49>) --- m_Cluster Multiplicity index on Cluster --- Dist Cluster distance class --- HRVc Cluster heliocentric radial velocity km/s n_HRVc Note on HRVc number=1 ': Cluster velocities recalculated with velocities of Markarian galaxies which are new members of clusters --- NGal Number of galaxies with published redshifts used to compute the mean HRV --- r_HRVc [A/E] References of the velocity of the cluster (See ref file) --- Mrk Markarian galaxy designation (see Cat. <VII/172>) --- HRVm Markarian galaxy heliocentric radial velocity km/s n_HRVm s for star --- z Redshift instead of radial velocity --- r_HRVm [1/14] References of the Markarian galaxy velocity (See ref file) --- Note *: individual notes number=2 Zw 0927.2+3446: The diameter of Mrk 399 is 0.30mm while the mean diameter for cluster galaxies is 0.60+/-0.12mm. Zw 1429.9+5256: The criterion of diameters was used. Mrk 816 may be a member of "distant" clusters Zw 1433.4+5335 or Zw 1435.0+5203. Zw 1552.5+3435: The velocity for the cluster in B-PPV was obtained with Mrk 493. Its a diameters is 1.05mm, while the mean diameter for cluster members is 0.34+/-0.10mm. --- Notes Notes --- All cases in which Markarian galaxy is positioned within the contours given in the Zwicky catalogue, but there are no velocities either for the cluster or for the galaxy or for either of them Cluster Cluster designation by right ascension and declination (1950) --- m_Cluster Multiplicity index on Cluster --- Dist Cluster distance class --- HRVc Cluster heliocentric radial velocity km/s n_HRVc Note on HRVc number=1 ': Cluster velocities recalculated with velocities of Markarian galaxies which are new members of clusters --- r_HRVc [A/E] References of the velocity of the cluster (See ref file) --- Mrk Markarian galaxy designation (see Cat. <VII/172>) --- u_Mrk Uncertainty flag on Mrk --- HRVm Markarian galaxy heliocentric radial velocity km/s r_HRVm [1/14] References of the Markarian galaxy velocity (See ref file) --- Note *: individual notes number=2 Zw 1043.9+5635: Mrk 35 (d=1.00mm) is a member of the group with V=1100km/s (B-PPV) and d=1.00mm, while the mean diameter for cluster galaxies is 0.38+/-0.16mm. --- Notes Notes --- Reference for velocities No Reference number or letter --- Name Author names ---- Bib Bibcode --- Cat Catalogue number --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_65_349.xml Spectral flux densities of radio sources at 22 MHz. J/A+AS/65/485 J/A+AS/65/485 22MHz flux densities of radio sources Spectral flux densities of radio sources at 22 MHz. R S Roger C H Costain D I Stewart Astron. Astrophys. Suppl. Ser. 65 485 1986 1986A&AS...65..485R J/AJ/74/366 : Flux densities at 22.25MHz. I. (Roger+, 1969) (obsoleted data) Radio sources galaxies: radio radio continuum: general radio sources: general table1 is a compilation of the flux densities at 22.25MHz for 395 sources, derived from three or more observations of each source. The source were measured over a period of several years with the T-shaped radiotelescope at the Dominion Astrophysical Observatory. The Note: This catalogue supersedes Cat. <J/AJ/74/366>
Flux densities at 22.25MHz Bname Name based on 1950 position --- RAh Right Ascension B1950 (hours) number=1 the position was added by Trushkin (1998) with CATS h RAm Right Ascension B1950 (minutes) number=1 the position was added by Trushkin (1998) with CATS min RAs Right Ascension B1950 (seconds) number=1 the position was added by Trushkin (1998) with CATS s DE- Declination B1950 (sign) number=1 the position was added by Trushkin (1998) with CATS --- DEd Declination B1950 (degrees) number=1 the position was added by Trushkin (1998) with CATS deg DEm Declination B1950 (minutes) number=1 the position was added by Trushkin (1998) with CATS arcmin DEs Declination B1950 (seconds) number=1 the position was added by Trushkin (1998) with CATS arcsec Source Source name --- S22MHz Flux density Jy e_S22MHz Mean error on S22MHz Jy o_S22MHz Number of observations --- Conf Name of confusing sources --- Bkg Name of background complexity --- Notes Notes number=2 the symbols have the following meaning: C: a 26.3 MHz flux density measured at Clark Lake is given by Viner and Erickson (1975AJ.....80..931V) G1, G2, G3, G4: Low frequency flux densities measured at Grakovo are given by Braude et al. (1978Ap&SS..54...37B, 1979Ap&SS..64...73B, 1981Ap&SS..74..409B, 1985Ap&SS.111..237B) respectively. 1: See notes for this source in Roger et al. (1973AJ.....78.1030R). 2: Comprises 3C66A and 3C66B and possibly a broad emission component. 3: Confusing sources surrounding 3C196 or emission from broad region centered on the source: near Abell 637. 4: Transits 0.8 min earlier than 4C14.31, near right ascension of Abell 795. 5: Evidence of E-W broadening. 6: Confused region; other sources not catalogued. Alternative interpretation with source on broad background feature gives a flux density of 128 +/- 20 Jy. 7: Broad emission centred on 3C298 (~50' EW). 8: Extended source, corrected for broadening. 9: Right ascension 45 sec later than listed in 4C (lobe shift ?). 10: Possibly extended. 11: Primary calibration source. 12: Confused region. 13: Epoch 1966.5. --- Patricia Bauer CDS 1999 Jun 21 UNKNOWN UNKNOWN # Corrections made by H.A. to the current electronic version: # 1157+734 3C268.1 had an 'X' in the notes column, shifted here to previous col. # 1857+129 3C394 closing bracket was added to (4C13.69) * 03-Dec-1998 Tables from the CATS data-base maintained by S. Trushkin (satr@ratan.sao.ru), at http://cats.sao.ru J_A+AS_65_485.xml Fully Sampled Neutral Hydrogen Survey of the Southern Milky Way J/A+AS/66/373 J/A+AS/66/373 Fully Sampled HI Survey of Southern Milky Way Fully Sampled Neutral Hydrogen Survey of the Southern Milky Way F J Kerr P F Bowers M Kerr P D Jackson Astron. Astrophys. Suppl. Ser. 66 373 1986 1986A&AS...66..373K H I data Interstellar matter Radio sources Surveys Galaxy: structure ISM: general The 18 m (60 foot) antenna of the CISRO at Parkes, Australia was used to completely sample the 21 cm line of neutral hydrogen over the Southern Milky Way. The survey covers Galactic longitudes l = 240 deg. to 350 deg, and Galactic latitudes |b| < 10 degrees, thus complementing the HI survey of Weaver and Williams (1973). The data are intended primarily for investigations of the global properties and structure of the Galaxy. Survey data are presented as brightness temperature maps which are gridded every 0.25 degrees in Galactic latitude and 0.5 degrees in Galactic longitude. The half-power beamwidth of the 18 m antenna is 48 arcmin and the velocity resolution of the survey is about 2.1 km/s. (The term "fully sampled" means that the observations are spaced sufficiently closely in sky position that observing a more closely spaced grid with the same antenna would not yield more information on the true sky distribution of the HI). The rms noise is about 0.27 K in the portions of the survey where the HI brightness temperature is low. The survey data are archived as 221 FITS-formatted files. Each file maps the brightness temperature at a fixed Galactic longitude onto the survey's chosen (V(LSR), Galactic latitude) grid. The files are named according to the Galactic longitude (e.g., l240p0 is the velocity-latitude map for longitude 240.0). The header record in each file gives the LSR velocity of the first channel; there are 300 channels, with a velocity step of 1 km/s between channels. There are data points with values less than -100.00 . These are flags which indicate missing or dropped data, and they should be ignored. Note that the brightness temperature scale of this survey is not the same as that of the Weaver & Williams HI Survey. If you wish to put both on the same scale, the longitude region from 240 through 250 can be used to obtain a scaling factor. Drs. Kerr and Jackson can also be contacted to obtain a scaling factor.
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J. Weiland ADF/ADC 1998 Oct 16 UNKNOWN UNKNOWN The survey data were obtained October 1998 from John Ohlmacher [UMd]. J_A+AS_66_373.xml CCD photometry in globular clusters. II. NGC 7492. J/A+AS/67/327 J/A+AS/67/327 CCD photometry in NGC 7492 CCD photometry in globular clusters. II. NGC 7492. R Buonanno C E Corsi I Ferraro F Fusi Pecci Astron. Astrophys. Suppl. Ser. 67 327 1987 1987A&AS...67..327B globular clusters: general stars: evolution stars: Population II CCD photometry in B,V colors of the globular cluster NGC 7492 (B1950 = 23 05.7 -15 54) is presented.
The photometry Star Running number in NGC 7492 --- Vmag from CCD mag B-V color index mag X position toward East arcsec Y position toward North arcsec Francois Ochsenbein CDS 1994 Oct 06 Ivan Ferraro <ivan@oarhp1.rm.astro.it> J_A+AS_67_327.xml An atlas and catalogue of northern dwarf novae J/A+AS/70/481 J/A+AS/70/481 An atlas and catalogue of northern dwarf nova An atlas and catalogue of northern dwarf novae A Bruch F J Fischer U Wilmsen Astron. Astrophys. Suppl. Ser. 70 481 1987 1987A&AS...70..481B dwarf novae finding charts novae, cataclysmic variables positions An atlas of 90 northern dwarf novae (delta greater than 20 deg) is presented. It is meant to supplement the Atlas of Southern and Equatorial Dwarf Novae of Vogt and Bateson (1982). Together, these publications represent a comprehensive collection of dwarf nova finding charts for the whole sky. In addition to the atlas, coordinates are given for most of the dwarf novae with accuracies significantly higher than published hitherto. (See J/A+AS/93/463 for the Southern Part)
Northern Dwarf Novae Name variable star name. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Epoch epoch of the coordinates. yr Francois Ochsenbein CDS 1993 Apr 13 J_A+AS_70_481.xml B and V photometry of faint stars in the Large Magellanic Cloud J/A+AS/73/37 J/A+AS/73/37 LMC faint stars BV photometry B and V photometry of faint stars in the Large Magellanic Cloud P Linde A Ardeberg H Lindgren G Lynga Astron. Astrophys. Suppl. Ser. 73 37 1988 1988A&AS...73...37L Magellanic Clouds Photometry Stars, faint electronography image crowding image processing Magellanic Clouds photometry, BV Photometric data on the Johnson BV system are given for 947 stars in a field close to the bar of the Large Magellanic Cloud. The data have been determined from electronographs calibrated through photoelectric photometry. The visual magnitudes of the programme stars range from V=14.63 to V=23.13.
Data for the measured stars. Seq Star sequential number number=1 Remark: Stars Nos. 90, 721, 751 and 835 have the following photoelectrically measured magnitudes: No. V B-V 90 16.63 1.74 721 15.25 0.62 751 13.56 0.72 835 17.35 1.40 --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Xpos X position number=2 1 pix = 0.144". pix Ypos Y position number=2 1 pix = 0.144". pix Vmag V magnitude mag B-V B-V colour index mag o_Vmag Number of observations in V magnitude --- n_Vmag Note on Vmag number=3 An * marks that the magnitude has been measured at an unusual intensity, in most cases lower than normal. --- o_Bmag Number of observations in B magnitude --- n_Bmag Note on Bmag number=3 An * marks that the magnitude has been measured at an unusual intensity, in most cases lower than normal. --- e_Vmag rms uncertainty on V magnitude mag e_Bmag rms uncertainty on B magnitude mag q_Vmag Quality factor on V magnitude number=4 5 denotes a perfect fit with no noticeable residuals and 1 a fit estimated as unsatisfactory. --- q_Bmag Quality factor on B magnitude number=4 5 denotes a perfect fit with no noticeable residuals and 1 a fit estimated as unsatisfactory. --- DeltaD Measure of positional accuracy arcsec Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 18 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_73_37.xml Survey at 327 MHz of the A 262 cluster region. J/A+AS/74/315 J/A+AS/74/315 327 MHz Survey of the A262 cluster region Survey at 327 MHz of the A 262 cluster region. G Righetti G Giovannini L Feretti Astron. Astrophys. Suppl. Ser. 74 315 1988 1988A&AS...74..315R Clusters, galaxy Galaxies, radio radio continuum: general radio sources: general surveys This catalog contains a survey at 327 MHz of the A262 cluster region. The survey was performed with the WSRT Telescope in the redundancy mode, and covers a circular region of 21 square degrees towards A262 (RA = 01h49m50s, decl = 35d54'20" -- B1950). The synthesized beam width is 56" x 93" (RA x DEC). 309 sources were detected, with a detection limit of 7 mJy (~5 sigma) at the field center. Nine of these galaxies have been identified with galaxies of the A262 cluster.
327 MHz Survey of Abell 262 Name Name of source number=1 This column contains the name of the source, consisting of the Westerbork survey number (73W) followed by a sequence number in order of right ascension. Source '73W076' is a double and both components are listed separately; '73W076a' and '73W076b'. --- RAh Right Ascension (B1950) (hour) number=2 These columns contain the B1950 source position. The positional accuracy depends on the source strength and size; it is estimated to be ~4" in right ascension and ~7" in declination for the weakest point sources, and becomes 2.4" and 4" respectively, for the sources with flux density > 14 mJy. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=2 These columns contain the B1950 source position. The positional accuracy depends on the source strength and size; it is estimated to be ~4" in right ascension and ~7" in declination for the weakest point sources, and becomes 2.4" and 4" respectively, for the sources with flux density > 14 mJy. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec r Distance from pointing center number=3 This column contains the distance from the pointing center, in degrees. This value is used to obtain the correction for primary beam attenuation. deg Smap Flux density measured on map number=4 The Smap column contains the source flux density, as measured on the map (in mJy). The Ssky column contains the source flux density corrected for the primary beam attenuation. The attenuation factor is calculated as f(r) = cos^-6^ * (21.154 * r) (ref. Oort, 1987), where 'r' is the distance from the pointing center, given above. mJy Ssky Flux density corrected for attenuation number=4 The Smap column contains the source flux density, as measured on the map (in mJy). The Ssky column contains the source flux density corrected for the primary beam attenuation. The attenuation factor is calculated as f(r) = cos^-6^ * (21.154 * r) (ref. Oort, 1987), where 'r' is the distance from the pointing center, given above. mJy tt Angular (DECONVOLVED or SKY) extent number=5 These columns give the angular extent, in arcsec (deconvolved), and the position angle, N to E, in degrees of the major axis of the radio brightness. arcsec pa Position angle N to E of major axis number=5 These columns give the angular extent, in arcsec (deconvolved), and the position angle, N to E, in degrees of the major axis of the radio brightness. deg ID Optical identification number=6 This column gives the optical identification of the source as follows: BO: Blue stellar object QSO: Quasar R: Red stellar object GAL: Galaxy EF: Empty field There are 227 empty fields, corresponding to 74% of the sample. The identification rate is independent of the flux density. Identifications are accepted when the positions agree to within 3 sigma (see text (1988A&AS...74..315R) for definition of sigma). --- oRA RA difference radio minus optical position number=7 These columns give the 'radio minus optical' positional difference between the radio and optical positions (RA and Dec, respectively), in arcsec. arcsec oDE Dec Difference radio minus optical position number=7 These columns give the 'radio minus optical' positional difference between the radio and optical positions (RA and Dec, respectively), in arcsec. arcsec Notes Notes number=8 This column marks notes on the optical identification. Due to the large uncertainty on the radio positions, a high contamination from chance coincidences is expected. For this reason, identifications with coincidence less than 2 sigma are differentiated from those between 2 and 3 sigma. The latter, which should be considered less reliable, are marked with an asterisk in this column. Where available, the name of the cluster galaxies is also given. --- Patricio Ortiz CDS 1999 Mar 30 UNKNOWN UNKNOWN "The catalogue was originally archived as A006 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_A+AS_74_315.xml A survey of an area around the North Ecliptic Pole at {lambda} 11 cm wavelength. J/A+AS/75/67 J/A+AS/75/67 Survey around the North Ecliptic Pole at 11 cm A survey of an area around the North Ecliptic Pole at {lambda} 11 cm wavelength. N Loiseau W Reich R Wielebinski P Reich W Munch Astron. Astrophys. Suppl. Ser. 75 67 1988 1988A&AS...75...67L Galaxies, radio north ecliptic pole radio continuum: general source catalog This catalog contains a survey of a rectangular area of 10x6 degrees in galactic coordinates (95.5{deg} < l < 101.5{deg} ; 28{deg} < b < 38{deg}) in the radio continuum in the direction of the north ecliptic pole (RA=18h, Dec=66.5{deg}) at 11.1 cm wavelength. The survey was conducted with the 100m radio telescope of the Max Planck Institut fur Radioastronomie. 469 sources were detected with an integrated flux density greater than 11 mJy, and with an angular resolution of 4.35'. The survey is believed to be complete to at least the 35 mJy level and can be used for comparison with deep surveys in other wavelengths of this area.
Survey Around the North Ecliptic Pole at 11 cm LRWR Sequential number of source number=1 This column gives the sequential number of the source. There are 469 sources contained in this survey. Source numbers are ordered by increasing right ascension. --- RA1950h Right Ascension (B1950) (hour) h RA1950m Right Ascension (B1950) (min) min RA1950s Right Ascension (B1950) (sec) s DE1950- Declination sign (B1950) --- DE1950d Declination (B1950) (deg) deg DE1950m Declination (B1950) (arcmin) arcmin DE1950s Declination (B1950) (arcsec) arcsec RAh Right Ascension (J2000) (hour) h RAm Right Ascension (J2000) (min) min RAs Right Ascension (J2000) (sec) s DE- Declination sign (J2000) --- DEd Declination (J2000) (deg) deg DEm Declination (J2000) (arcmin) arcmin DEs Declination (J2000) (arcsec) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg S2695 Integrated flux density at 2695 MHz number=2 This column gives the integrated 2695 MHz (11.1 cm) flux density in mJy. Sources were fitted by procedures described in Reich et al. (1984A&AS...58..197R), where two Gaussian fits were made along the major and minor axis of an ellipse which fitted the source structure. Parameters of these fits are given in the size column described below. mJy size Apparent size and PA of source number=3 This column gives the apparent source size as measured with a Gaussian beam (HPBW = 4.35' +/- 0.1'). The following abbreviations are used: PL = point-like source, e.g. smaller than 4.5'x4.5' SE = slightly extended source, e.g. smaller than 5'x5' ** = uncertain parameters. Note: When these symbols are used, they are given in the middle of the 12-character field. In case of extended sources, large and small axis are listed in arcmin and the position angle of the large axis in Galactic coordinates is given. arcmin err_code Error class of the fitting procedure number=4 A four-digit code describing the error class of the fitting procedure is given in this column as follows: 1st digit: positional error in units of 10" 2nd digit: flux density error in units of 10% 3rd digit: size error in units of 20" 4th digit: error of the position angle in 5 degrees --- Patricio Ortiz CDS 1999 Mar 30 UNKNOWN UNKNOWN "The catalogue was originally archived as A008 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_A+AS_75_67.xml UBV and uvbyb photometry of stars in the region of the Zeta Sculptoris cluster J/A+AS/76/101 J/A+AS/76/101 UBV and uvbyb in zeta Scl cluster UBV and uvbyb photometry of stars in the region of the Zeta Sculptoris cluster B E Westerlund R Garnier K Lundgren B Pettersson J Breysacher Astron. Astrophys. Suppl. Ser. 76 101 1988 1988A&AS...76..101W open clusters and asociations: individual (zeta Scl) photometry: UBV photometry: uvby, beta stars: metal-deficient 130 stars in the region of the Zeta Sculptoris cluster have been observed photoelectrically, most of them in UBVBeta and about half of them in uvby and a few also in the Cousins' system.
Photometric data for the stars in the cluster area N Identification number --- n_N * = stars considered to be members of the cluster --- CoD Cordoba Durchmusterung denomination --- Ep Epstein's Number (Epstein I., 1968, Astron. J., 73, 556) --- HD HD number --- Sp Spectral type --- Vmag V magnitude mag B-V B-V colour mag U-B U-BV colour mag o_Vmag Number of UBV observations --- b-y b-y colour mag m1 m1 index mag c1 c1 index mag u-b u-b colour mag o_b-y Number of uvby observations --- Beta Beta index mag o_Beta Number of Beta observations --- SpBeta Spectral type from Beta index ---- Patricia Bauer CDS 1994 Oct 06 J_A+AS_76_101.xml Photographic UBV photometry to V~21 in the Puppis window J/A+AS/77/447 J/A+AS/77/447 Puppis window UBV photometry Photographic UBV photometry to V~21 in the Puppis window B C Reed Astron. Astrophys. Suppl. Ser. 77 447 1989 1989A&AS...77..447R Galaxy: stellar content OB association photometry surveys Photographic UBV photometry of 1302 stars in a 76 square-arcminute field in the Puppis window to U~16.9, (B, V)~21 is presented. The presence of an OB association at r~6kpc in this direction as reported by Stetson and FitzGerald (1985) is confirmed. No evidence of any more distant early-type stars is indicated.
Blue stars in MW 245 Id Identification number to the charts --- n_Id * indicates double or multiple image --- E(B-V) Reddening mag e_E(B-V) rms uncertainty on E(B-V) mag V0-MV Absolute distance modulus --- e_V0-MV rms uncertainty on V0-MV --- UBV photometry Id Identification number to the charts --- Vmag V magnitude mag B-V B-V color index mag U-B U-B color index mag o_Vmag Number of measurements in V band --- o_Bmag Number of measurements in B band --- o_Umag Number of measurements in U band --- e_Vmag rms uncertainty on V magnitude mag e_Bmag rms uncertainty on B magnitude mag e_Umag rms uncertainty on U magnitude mag Note Notes number=1 1: crowed image where an effort was made to measure each star individually 2: double 3: faint companion nearby 4: possible galaxy 5: secondary image --- Simona Mei, Patricia Bauer CDS 1995 Feb 27 UNKNOWN UNKNOWN Keypunched at CDS J_A+AS_77_447.xml New proper-motion stars south of declination -40deg and right ascension between 00h00 and 04h30 J/A+AS/78/231 J/A+AS/78/231 New proper-motion stars Dec<-40, 0<RA<4h30 New proper-motion stars south of declination -40deg and right ascension between 00h00 and 04h30 H Wroblewski C Torres Astron. Astrophys. Suppl. Ser. 78 231 1989 1989A&AS...78..231W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/91/129 : Dec<-40, 0<RA<4h30, stars 145 to 521 (Wroblewski+ 1991) J/A+AS/105/179 : Dec<-40, 16<RA<24h, stars 522 to 1069 (Wroblewski+ 1994) J/A+AS/115/481 : -30<Dec<-5, 0<RA<9h, stars 1070 to 1563 (Wroblewski+ 1996) J/A+AS/83/317 : LTT stars, Dec<-40, 0<RA<4h30 (Wroblewski+ 1990) J/A+AS/92/449 : LTT stars, Dec<-40, 4h30<RA<16h (Wroblewski+ 1992) J/A+AS/110/27 : LTT stars, Dec<-40, 16<RA<24h (Wroblewski+, 1995) Proper motions astrometry proper motions Data are given for 144 new proper-motion stars with {mu}>=0.15arcsec/yr.
Stars 1/144 WT Running number --- Loc Localisation (area and number) --- mpg Photographic magnitude, accurate to 0.5mag mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RAh2000 Right Ascension 2000 (hours) h RAm2000 Right Ascension 2000 (minutes) min RAs2000 Right Ascension 2000 (seconds) s DE-2000 Declination 2000 (sign) --- DEd2000 Declination 2000 (degrees) deg DEm2000 Declination 2000 (minutes) arcmin DEs2000 Declination 2000 (seconds) arcsec pm Total proper motion arcsec/yr e_pm Mean error on pm arcsec/yr pmPA Position angle (North to East) of the proper motion in J2000 equinox deg Remark Remarks number=1 '4' when proper-motion is the mean of #4 pairs of plates (*), '6' when proper-motion is the mean of #6 pairs (**). --- James Marcout, Francois Ochsenbein CDS 1994 Feb 22 UNKNOWN UNKNOWN Keypunched at CDS in February 1994 J_A+AS_78_231.xml Spectroscopy of 1 Jy and S5 radio source Identifications. I. J/A+AS/80/103 J/A+AS/80/103 Spectroscopy of 1 Jy and S5 radio source Id. I. Spectroscopy of 1 Jy and S5 radio source Identifications. I. M Stickel J W Fried H Kuehr Astron. Astrophys. Suppl. Ser. 80 103 1989 1989A&AS...80..103S BL Lacertae objects: general galaxies: active galaxies: distances and redshifts optical spectroscopy quasars: general radio sources: general Optical spectroscopy is reported for a number of flat spectrum radio sources, most of which are either classified as BL Lacertae objects or have been described as BL Lac candidates. A total of ten new redshifts are presented. The suggested redshifts for three objects are confirmed and spectroscopic data are given for eight additional objects with already known redshifts. A variety of emission features and emission line strengths is found reaching from strong lines characteristic for high redshift quasars to very weak lines typical for classical BL Lac objects.
Observed radio source identifications Object Object name number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) --- RAh Right Ascension 1950 (hours) number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) h RAm Right Ascension 1950 (minutes) number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) min RAs Right Ascension 1950 (seconds) number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) s DE- Declination 1950 (sign) number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) --- DEd Declination 1950 (degrees) number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) deg DEm Declination 1950 (minutes) number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) arcmin DEs Declination 1950 (seconds) number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) arcsec m1 brightest magnitude of the optical identification number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) mag m2 faintest magnitude of the optical identification number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) mag fc References to published Finding Charts --- ref References to other compilations --- Names Other names number= >1. Edwards et al. (1975) >2. Hunstead and Jauncey (1970) >3. Veron and Veron (1975) >4. Cohen et al. (1977) >5. Kuehr (1977) >6. Craine and Price (1976) >7. Arp et al. (1976) >8. Hoskins et al. (1974) >9. Bolton et al. (1975) >10. Walter and West (1980) >11. Nicolson et al. (1979) >12. Folsom et al. (1970) >13. Kapahi (1979) >14. Radivich and Kraus (1971) >15. Peterson et al. (1976) >16. Savage and Wall (1976) >17. Condon et al. (1977) >18. Kuehr et al. (1987) >19. Craine et al. (1976) >20. Peterson and Bolton (1973) >21. Fugmann (1988) >22. Lue (1970) >23. Savage and Bolton (1977) >24. Browne et al. (1973) >25. Blake (1970) >26. Smith et al. (1985) >27. Fugmann et al. (1988) >28. Morton and Tritton (1982) >29. Veron et al. (1976) >30. Burbidge and Hewitt (1987) >31. Hewitt and Burbidge (1987) >32. Ledden and O'Dell (1985) >33. Impey and Neugebauer (1988) >34. Wall and Peacock (1985) >35. Veron-Cetty and Veron (1987) --- Journal of the observations Object Object name --- Tel Telescope: CA 3.5 = 3.5 m telescope on Calar Alto, Spain LS 2.2 = 2.2 m telescope on La Silla, Chile --- Date Observation date --- iTime Total Integration time s Scale Scale of the wavelength calibrated spectra 0.1nm/pix Line data Object Object name --- z Redshift computed from unweighted z_ind --- AltId "a" indicates an alternative identification --- Id Element identification --- lam_0 Rest wavelength 0.1nm lam_obs Observed wavelength 0.1nm z_ind Individual redshift --- FWHM FWHM (for emission line) 0.1nm EW Equivalent width (for emission line) 0.1nm Flux Flux (10-16erg/s/cm2) 10-19W/m2 Rem abs = intervening absorption line system --- CDS 1993 Nov 12 J_A+AS_80_103.xml IRAS sources beyond the solar circle. I. CO observations J/A+AS/80/149 J/A+AS/80/149 IRAS sources beyond the solar circle. I. CO obs IRAS sources beyond the solar circle. I. CO observations J G A Wouterloot J Brand Astron. Astrophys. Suppl. Ser. 80 149 1989 1989A&AS...80..149W ICO(1-0) emission kinematic distances luminosities *** No Description Available ***
IRAS Abstract: C-12O (J = 1-0) has been observed with the 15-m SEST and the 30-m IRAM telescope in the direction of 1302 IRAS sources with colors of star forming regions located within 10 deg of the galactic plane in the interval between 85 and 280 deg. Emission components with line profiles that are non-Gaussian (showing, e.g., possible self-absorption or wings) are identified; this information may serve as a basis for selecting sources for future research. For all components, kinematic heliocentric and galactocentric distances, and distances from the galactic plane are derived. For those components which may be associated with the IRAS sources, bolometric luminosities are derived. These data will be analyzed and compared with HI data in subsequent papers.
CO (J=1-0) line parameters and derived distances and luminosities of IRAS sources NUMBER Running number --- IRAS IRAS source name --- GLON Galactic longitude number=1 Due to the removal of some small bugs in our programs, and other errors, there can be a difference of +/-0.01 degree in l, +/-0.01 kpc in R and d, +/-1 pc in z and +/- 0.1 in L_IR compared to the publication. deg GLAT Galactic latitude deg Tel I = source observed at IRAM S = source observed at SEST G = source observed at Gornergrat CO(3-2) --- rms n when no line detected; T_A* contains rms in this case --- T_A* Antenna temperature number=2 For source 1045 there are no values for T, V, dV because there is very broad emission which is not measurable with frequency switching (Remark in paper). K e_TA Uncertainty in T_A* K Vlsr Velocity number=2 For source 1045 there are no values for T, V, dV because there is very broad emission which is not measurable with frequency switching (Remark in paper). km/s e_Vlsr Uncertainty in Vlsr km/s DV Line width number=2 For source 1045 there are no values for T, V, dV because there is very broad emission which is not measurable with frequency switching (Remark in paper). km/s e_DV Uncertainty in DV km/s Rem Remarks, as: ft = flat top at = asymmetric top blue (bat) / red (rat) a = asymmetry blue (ba) / red (ra) w = wing blue (bw) / red (rw) s = shoulder blue (bs) / red (rs) cs = complex spectrum eir= emission in ref. sa = self-absorption R = remark in the publication * = observed with 30" offset in Azimuth. --- R Kinematic galactocentric distance (1) from (theta/220km/s)=(R/8.5kpc)**0.0382 kpc r_R 'f' for forbidden velocities '>' R uncertain; put at 25 kpc. --- d Kinematic heliocentric distance (1). d=0.1 kpc taken for sources with forbidden velocities in quadrant 2,3, and if formula gives d<0.1kpc. kpc z Distance from galactic plane (1). pc L_IR Total infrared luminosity (1); only given for component associated with IRAS source. Sun Ident Identifications. (f) means that associated object is further than 100" from IRAS position. --- CDS 1999 Jan 00 J_A+AS_80_149.xml Meter wavelength structures, flux densities and accurate positions of weak radio sources. J/A+AS/80/215 J/A+AS/80/215 Lunar occultations of weak radio sources Meter wavelength structures, flux densities and accurate positions of weak radio sources. C E Akujor M N Joshi I Kazes Astron. Astrophys. Suppl. Ser. 80 215 1989 1989A&AS...80..215A Radio continuum Radio lines Radio sources catalogs occultations radio spectrum weak radio sources: general This catalog contains the results of lunar occultation observations of 106 radio sources within declination +/- 19 degrees at 327 MHz. There are 171 sources listed in the catalog due to multiple components for some of the radio sources. Flux densities were measured at 327 MHz by lunar occultation with the Ooty Telescope. Flux densities have also been measured at 18 cm (1669 MHz) and 21 cm (1413 MHz) using the Nancay telescope. Optical identifications on the basis of the radio positions and angular structures are given. This catalog is a merge of table 1 and table 2 from the publication.
Radio Source Parameters From Lunar Occultation, Observations (-19{deg} to 19{deg}) Name Name of source number=1 The Name column gives the radio source name. The IAU designation is used throughout. The Oname (other name) column gives the most common name of the radio source from other catalogs, such as 4C, MG, PKS etc. Some corrections were made to the data in order that the source names were consistent between the two tables. --- Note * if a note on the source in the paper number=2 The 'Note' column is marked with an asterisk if there are comments or notes on the source in the published paper. The 'comp' column gives the individual component name if the source shows more than a single structure. A 'CN' in this column means the position is that of the radio centroid. --- comp Component of source number=2 The 'Note' column is marked with an asterisk if there are comments or notes on the source in the published paper. The 'comp' column gives the individual component name if the source shows more than a single structure. A 'CN' in this column means the position is that of the radio centroid. --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s e_RAs Error on RA s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec e_DEs Error on Dec arcsec S327 Flux density at 327 MHz number=3 These columns give flux densities and errors at 327 MHz, 1413 MHz, and 1669 MHz. All flux density measurements are in Jy. The 327 MHz flux densities are from the Ooty telescope; the 1413 MHz and 1669 MHz flux densities are from the dual-reflector Nancay Telescope. Errors include contributions from the integration of the different observation cycles for each channel, the integration of the channels for each wavelength, and contributions from conversion to flux densities using calibrator fluxes. Flux densities were measured on the scale of Baars, et al. (1977A&A....61...99B). One 327 flux density was changed to make it consistent with table 2 of the published paper. See details under "History:" below. Jy e_S327 Error on 327 flux density number=3 These columns give flux densities and errors at 327 MHz, 1413 MHz, and 1669 MHz. All flux density measurements are in Jy. The 327 MHz flux densities are from the Ooty telescope; the 1413 MHz and 1669 MHz flux densities are from the dual-reflector Nancay Telescope. Errors include contributions from the integration of the different observation cycles for each channel, the integration of the channels for each wavelength, and contributions from conversion to flux densities using calibrator fluxes. Flux densities were measured on the scale of Baars, et al. (1977A&A....61...99B). One 327 flux density was changed to make it consistent with table 2 of the published paper. See details under "History:" below. Jy S1413 Flux density at 1413 MHz number=3 These columns give flux densities and errors at 327 MHz, 1413 MHz, and 1669 MHz. All flux density measurements are in Jy. The 327 MHz flux densities are from the Ooty telescope; the 1413 MHz and 1669 MHz flux densities are from the dual-reflector Nancay Telescope. Errors include contributions from the integration of the different observation cycles for each channel, the integration of the channels for each wavelength, and contributions from conversion to flux densities using calibrator fluxes. Flux densities were measured on the scale of Baars, et al. (1977A&A....61...99B). One 327 flux density was changed to make it consistent with table 2 of the published paper. See details under "History:" below. Jy e_S1413 Error on 1413 flux density number=3 These columns give flux densities and errors at 327 MHz, 1413 MHz, and 1669 MHz. All flux density measurements are in Jy. The 327 MHz flux densities are from the Ooty telescope; the 1413 MHz and 1669 MHz flux densities are from the dual-reflector Nancay Telescope. Errors include contributions from the integration of the different observation cycles for each channel, the integration of the channels for each wavelength, and contributions from conversion to flux densities using calibrator fluxes. Flux densities were measured on the scale of Baars, et al. (1977A&A....61...99B). One 327 flux density was changed to make it consistent with table 2 of the published paper. See details under "History:" below. Jy S1669 Flux density at 1669 MHz number=3 These columns give flux densities and errors at 327 MHz, 1413 MHz, and 1669 MHz. All flux density measurements are in Jy. The 327 MHz flux densities are from the Ooty telescope; the 1413 MHz and 1669 MHz flux densities are from the dual-reflector Nancay Telescope. Errors include contributions from the integration of the different observation cycles for each channel, the integration of the channels for each wavelength, and contributions from conversion to flux densities using calibrator fluxes. Flux densities were measured on the scale of Baars, et al. (1977A&A....61...99B). One 327 flux density was changed to make it consistent with table 2 of the published paper. See details under "History:" below. Jy e_S1669 Error on 1669 flux density number=3 These columns give flux densities and errors at 327 MHz, 1413 MHz, and 1669 MHz. All flux density measurements are in Jy. The 327 MHz flux densities are from the Ooty telescope; the 1413 MHz and 1669 MHz flux densities are from the dual-reflector Nancay Telescope. Errors include contributions from the integration of the different observation cycles for each channel, the integration of the channels for each wavelength, and contributions from conversion to flux densities using calibrator fluxes. Flux densities were measured on the scale of Baars, et al. (1977A&A....61...99B). One 327 flux density was changed to make it consistent with table 2 of the published paper. See details under "History:" below. Jy Sp-Index Spectral index between 327 and 1669 MHz number=4 This column gives the spectral index between 327 MHz and 1669 MHz. 1413 MHz flux densities are used where there is no measurement at 1669 MHz. Alpha is defined as S {prop.to} nu^{(-alpha)}^. --- PosAng_i Position angle of scan in immersion occultation number=5 The PosAng_i column gives the position angle (in degrees) of scan in immersion occultation. The Beta_i column gives the effective resolution achieved along the position angle given by PosAng_i. The Size_i column gives the derived angular size of the whole source or an individual component along the position angle given by PosAng_i and with effective resolution given by Beta_i. The PosAng_e, Beta_e, and Size_e columns give these same quantities, but for another scan corresponding to occultation emersion. deg Beta_i Effective resolution achieved along immersion PA number=5 The PosAng_i column gives the position angle (in degrees) of scan in immersion occultation. The Beta_i column gives the effective resolution achieved along the position angle given by PosAng_i. The Size_i column gives the derived angular size of the whole source or an individual component along the position angle given by PosAng_i and with effective resolution given by Beta_i. The PosAng_e, Beta_e, and Size_e columns give these same quantities, but for another scan corresponding to occultation emersion. arcsec Size_i Derived angular size of source or comp in immersion number=5 The PosAng_i column gives the position angle (in degrees) of scan in immersion occultation. The Beta_i column gives the effective resolution achieved along the position angle given by PosAng_i. The Size_i column gives the derived angular size of the whole source or an individual component along the position angle given by PosAng_i and with effective resolution given by Beta_i. The PosAng_e, Beta_e, and Size_e columns give these same quantities, but for another scan corresponding to occultation emersion. arcsec PosAng_e Position angle of scan in emersion occultation number=5 The PosAng_i column gives the position angle (in degrees) of scan in immersion occultation. The Beta_i column gives the effective resolution achieved along the position angle given by PosAng_i. The Size_i column gives the derived angular size of the whole source or an individual component along the position angle given by PosAng_i and with effective resolution given by Beta_i. The PosAng_e, Beta_e, and Size_e columns give these same quantities, but for another scan corresponding to occultation emersion. deg Beta_e Effective resolution achieved along emersion PA number=5 The PosAng_i column gives the position angle (in degrees) of scan in immersion occultation. The Beta_i column gives the effective resolution achieved along the position angle given by PosAng_i. The Size_i column gives the derived angular size of the whole source or an individual component along the position angle given by PosAng_i and with effective resolution given by Beta_i. The PosAng_e, Beta_e, and Size_e columns give these same quantities, but for another scan corresponding to occultation emersion. arcsec Size_e Derived angular size of source or comp in emersion number=5 The PosAng_i column gives the position angle (in degrees) of scan in immersion occultation. The Beta_i column gives the effective resolution achieved along the position angle given by PosAng_i. The Size_i column gives the derived angular size of the whole source or an individual component along the position angle given by PosAng_i and with effective resolution given by Beta_i. The PosAng_e, Beta_e, and Size_e columns give these same quantities, but for another scan corresponding to occultation emersion. arcsec LAS Largest angular size number=6 These columns give information on the overall radio structure of the source. The largest angular size is given (in arcseconds) in the last column; the corresponding position angle of the major axis (in degrees) is given in the 'Maj_PA' column; and the source structure is described in the 'struct' column as follows: D double PD probable double U unresolved T triple HT head-tail Ext indication of extended feature CH core-halo Cx complex Br emission bridge with percentage of flux contained ? indicated structure is not very certain arcsec Maj_PA Position angle of the major source axis number=6 These columns give information on the overall radio structure of the source. The largest angular size is given (in arcseconds) in the last column; the corresponding position angle of the major axis (in degrees) is given in the 'Maj_PA' column; and the source structure is described in the 'struct' column as follows: D double PD probable double U unresolved T triple HT head-tail Ext indication of extended feature CH core-halo Cx complex Br emission bridge with percentage of flux contained ? indicated structure is not very certain deg struct Source structure description number=6 These columns give information on the overall radio structure of the source. The largest angular size is given (in arcseconds) in the last column; the corresponding position angle of the major axis (in degrees) is given in the 'Maj_PA' column; and the source structure is described in the 'struct' column as follows: D double PD probable double U unresolved T triple HT head-tail Ext indication of extended feature CH core-halo Cx complex Br emission bridge with percentage of flux contained ? indicated structure is not very certain --- oRA Radio minus optical offset in RA number=7 These columns give the radio-minus-optical offset in right ascension and declination, in arcseconds. The optical positions are accurate to ~0.5". arcsec oDE Radio minus optical offset in Dec number=7 These columns give the radio-minus-optical offset in right ascension and declination, in arcseconds. The optical positions are accurate to ~0.5". arcsec Pmag Photographic magnitude of optical object number=8 This column gives the photographic magnitude of the optical object, estimated from PSS prints based on the calibrations of King and Raff (1977). The uncertainties are generally ~+/- 1 magnitude. mag ID Optical object in field number=9 This column gives the optical object in the field or an abbreviation describing the nature of the field. The following abbreviations are used: EF empty field BSO blue stellar object RSO red stellar object NSO neutral stellar object QSO quasi-stellar object G galaxy BG blue galaxy RG red galaxy CWD crowed field INP identification not possible for technical reasons ID attached to the abbreviation means positive or likely identification and '?' means identification given is uncertain. x) refer to references for published optical charts as follows: a) Hunstead & Jauncey 1970, MNRAS 149, 91. b) Wills & Wills 1979. (1979ApJS...41..689W) Lawrence et al.1986. (1986ApJS...61..105L) c) Bolton et al. 1981, AuJP 34, 445. (1981AuJPh..34..445B) d) Wills & Bolton 1969. (1969AuJPh..22..775W) e) Lawrence et al. 1986. (1986ApJS...61..105L) f) Bolton & Wall 1970, AuJP 23, 789. g) Kapahi et al. 1973. (1973AJ.....78..673K) --- |b| Galactic latitude of radio source (|b|) number=10 This column gives the absolute value of the galactic latitude, |b| of the radio source, in integer degrees. deg Oname Most common names of source number=1 The Name column gives the radio source name. The IAU designation is used throughout. The Oname (other name) column gives the most common name of the radio source from other catalogs, such as 4C, MG, PKS etc. Some corrections were made to the data in order that the source names were consistent between the two tables. --- Patricio Ortiz CDS 1999 Mar 30 UNKNOWN UNKNOWN "The catalogue was originally archived as A042 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." The following changes were made to tables 1 and 2, based on flux comparisons and comparisons with IAU names. Table 1: 1. changed 0408+169 to 0408+160 to accurately reflect position 2. changed 1313-006 to 1313-066 to accurately reflect position 3. changed dec from -171352.6 to -175352.6 for 1659-178 (texas position) 4. changed 1923-187 to 1823-187 to accurately reflect position 5. changed the 327 flux for 1750-187 from 0.4 to 0.25 so that it would agree with the value in table 2 (and therefore alpha would be correct). Table 2: 1. changed 0031+041 to 0035+041 to agree with table 1 2. changed 0323+152 to 0324+153 to agree with table 1 3. changed 0324+153 to 0324+152 to agree with table 1 4. changed 0408+169 to 0408+160 to accurately reflect position 5. changed 0601+158 to 0601+185 to agree with table 1 6. changed 0743+161 to 0742+161 to agree with table 1 7. removed this line as it has no corresponding source in table 1 probably an incorrect combination of 0743+161 (now changed) and 0746+162: 0743+162 0.45 .04 0.53 .06 -0.11 8. changed 1105+037 to 1105+037a to agree with table 1 9. changed 1214-029 (flux=0.55) to 1214-029a to agree with table 1 10. changed 1214-029 (flux=0.45) to 1214-029b to agree with table 1 11. changed 1313-006 to 1313-066 to accurately reflect position 12. changed 2106-130 to 2106-130a to agree with table 1 --C. Stern Grant 16 Jun 1993 13. 1406-102 B 140663.00 0.05 -101157.9 1.0 0.35 was changed to: 1406-102 B 140646.30 0.05 -101157.9 1.0 0.35 |||| as a likely correction to the excessive value of 63 in the seconds of RA (the mean value is 45.48) P. Ortiz, 12 Apr 1999 J_A+AS_80_215.xml Deep photometry of globular clusters. XII. The metal-poor clusters NGC 5694 and Terzan 8 J/A+AS/82/71 J/A+AS/82/71 Deep photometry of NGC 5694 and Terzan 8 Deep photometry of globular clusters. XII. The metal-poor clusters NGC 5694 and Terzan 8 S Ortolani R Gratton Astron. Astrophys. Suppl. Ser. 82 71 1990 1990A&AS...82...71O globular clusters: general stars: photometry We present deep CCD photometries for the little known metal-poor clusters NGC 5694 and Terzan 8 down to V~24. NGC 504 has a blue horizontal branch, a very high radial velocity, a metallicity of [Fe/H]=-1.65+/-0.06, a reddening of E(B-V)=0.10+/-0.03, and an apparent distance modulus of (m-M)_v_=17.82+/-0.15. It is located at 26.0+/-1.8kpc from the galactic center. The helium content derived from the ratio between the number of stars on the horizontal branch and the giant and asymptotic giant branches is consistent with that obtained for other clusters. Terzan 8 is a metal-poor ([Fe/H]=-1.81+/-0.10) moderately reddened (E(B-V)=0.20+/-0.05) cluster with a blue horizontal branch and apparent distance modulus of (m-M)_v_=17.25+/-0.15. It is located at 13.8+/-2.0 kpc from the galactic center. The c-m diagram and the luminosity function of NGC 5694 and Terzan 8 are similar to the M92 ones. NGC 5694 and Terzan 8 have ages close to that of the "classical" globular cluster M92.
NGC 5694 photometry Star Star number --- Xpos X position pix Ypos Y position pix Vmag V magnitude mag e_Vmag Error on V magnitude mag B-V B-V colour index mag e_B-V Error on B-V mag Note Note number=1 When '2' star is rejected using criteria described in Sect. 4.1 of the paper --- Terzan 8 photometry Star Star number --- Xpos X position pix Ypos Y position pix Vmag V magnitude mag B-V B-V colour index mag Note Note number=1 1: star measured on both frames 2: star measured on frame 2 only 3: star measured on frame 1 only --- Marie-Jose Wagner, Simona Mei CDS 1995 Mar 13 UNKNOWN UNKNOWN Keypunched at CDS J_A+AS_82_71.xml New proper motion determination of Luyten catalogue stars (LTT) south of declination -40 and right ascension between 00h 30m. J/A+AS/83/317 J/A+AS/83/317 New proper-motion LTT stars Dec<-40, 0<RA<4h30 New proper motion determination of Luyten catalogue stars (LTT) south of declination -40 and right ascension between 00h 30m. H Wroblewski C Torres Astron. Astrophys. Suppl. Ser. 83 317 1990 1990A&AS...83..317W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/78/231 : Dec<-40, 0<RA<4h30, stars 1 to 144 (Wroblewski+ 1989) J/A+AS/91/129 : Dec<-40, 0<RA<4h30, stars 145 to 521 (Wroblewski+ 1991) J/A+AS/105/179 : Dec<-40, 16<RA<24h, stars 522 to 1069 (Wroblewski+ 1994) J/A+AS/115/481 : -30<Dec<-5, 0<RA<9h, stars 1070 to 1563 (Wroblewski+ 1996) J/A+AS/92/449 : LTT stars, Dec<-40, 4h30<RA<16h (Wroblewski+ 1992) J/A+AS/110/27 : LTT stars, Dec<-40, 16<RA<24h (Wroblewski+, 1995) Luyten W.J. 1957, A Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motions Exceeding 0.2 arcsec Annualy (The Lund Press, Minneapolis, Minnesota). Luyten W.J. 1979, LHS Catalogue, University of Minnesota, Minneapolis, Minnesota. (Cat. <I/87>) Proper motions astrometry proper motions Data are given for 104 LTT stars found on 11 areas, covering 25 squares degrees each, south of declination -40deg and right ascension between 00h and 04h30m. Three stars present differences in proper motion >0.10", six present differences in position angle >=20deg and one presents those differences in both values.
Positions and relative proper motions Seq Running number --- LTT Star number in Luyten's catalogue --- Loc Localisation (area and number) --- mpg Photographic magnitude, accurate to 0.5mag mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RAh2000 Right Ascension 2000 (hours) h RAm2000 Right Ascension 2000 (minutes) min RAs2000 Right Ascension 2000 (seconds) s DE-2000 Declination 2000 (sign) --- DEd2000 Declination 2000 (degrees) deg DEm2000 Declination 2000 (minutes) arcmin DEs2000 Declination 2000 (seconds) arcsec pm Total proper motion arcsec/yr e_pm Mean error on pm arcsec/yr pmPA Position angle (North to East) of the proper motion in J2000 equinox deg Dpm Difference LTT pm minus pm (this work) number=1 It can be seen that most proper motions given in LTT are larger than those determined by us. It is important to point out that stars 26 (LTT 703), 54 (LTT 1323), 73 (LTT 1679) and 80 (LTT 1765) show considerable differences (>0.10") arcsec Remaks Remarks number=2 '4' when proper-motion is the mean of #4 pairs of plates. '1' when LTT and present PA value differ by 20deg or more. Stars 26 (LTT 703), 30 (LTT 932), 35 (LTT 1019), 48 (LTT 1129), 60 (LTT 1403) and 71 (LTT 1634), show values of position angles that differ by 20deg or more. The case of star 60 (LTT 1403) is remarkable for which Lyuten estimates a position angle of 320deg, while our results is 37deg. --- James Marcout, Patricia Bauer CDS 1997 Mar 13 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_83_317.xml The Effelsberg 21cm radio continuum survey of the Galactic plane between l=357deg and l=95.5deg J/A+AS/83/539 J/A+AS/83/539 21cm radio continuum survey. I. The Effelsberg 21cm radio continuum survey of the Galactic plane between l=357deg and l=95.5deg W Reich P Reich E Furst Astron. Astrophys. Suppl. Ser. 83 539 1990 1990A&AS...83..539R J/A+AS/126/413 : 21cm radio continuum survey. II. (Reich+ 1997) Radio sources Galactic radio emission radio continuum: general radio sources: general The results of a radio continuum survey at 21 cm wavelength of the Galactic plane between 357 and 95.5deg and -4 to 4deg carried out with the Effelsberg 100-m radio telescope. The data have been absolutely calibrated by using the Stockert northern sky survey at the same wavelength. Contour maps are shown with a sensitivity of 61.6mJy/beam area at an angular resolution (HPBW) of 94. In addition, a list of 884 compact objects with peak flux densities greater than 98 mJy and apparent sizes less than 16 arcsec is presented.
List of 884 small diameter radio sources No Source number --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec RA2000d Right ascension (J2000.0) h RA2000m Right ascension (J2000.0) min RA2000s Right ascension (J2000.0) s DE2000- Declination sign --- DE2000d Declination (J2000.0) deg DE2000m Declination (J2000.0) arcmin DE2000s Declination (J2000.0) arcsec Sint Integrated flux density Jy SPeak Peak flux density mJy MajAxis Major axis of gaussian arcmin --- --- MinAxis Minor axis of gaussian arcmin --- --- PA Galactic position angle of the ellipsoid deg Size Point-like sources or slightly extended sources number=1 PL = point-like sources, major axis x minor axis of gaussian <10x10arcmin^2^ SE = slightly extended sources, major axis x minor axis of gaussian <11x11arcmin^2^ --- e_Pos Positional error 10arcsec e_Sint Integrated flux density error 10% e_MajAxis Size error (on MajAxisand MinAxis) 20arcsec e_PA Error of the position angle 3deg Patricia Bauer CDS 1997 Dec 08 Patricia Reich <preich@mpifr-bonn.mpg.de> J_A+AS_83_539.xml CCD-photometry of the galactic globular cluster NGC 2808. J/A+AS/84/59 J/A+AS/84/59 Photometry NGC 2808 CCD-photometry of the galactic globular cluster NGC 2808. F R Ferraro G Clementini F Fusi Pecci R Buonanno G Alcaino Astron. Astrophys. Suppl. Ser. 84 59 1990 1990A&AS...84...59F globular clusters: general Hertzsprung-Russell (HR diagram) photometry: CCD stars: evolution B,V CCD photometry is reported for 5724 stars in the globular cluster NGC 2808. The morphology of the color-magnitude diagram confirms the results presented by Harris (1974, 1975, and 1978). In particular, the peculiar wide gap detected on the horizontal branch is still present; however, it seems more a region of scarce population rather than a zone of avoidance.
CCD data Photographic data N Identification number --- Vmag V magnitude mag B-V B-V magnitude mag X X position pix Y Y position pix Patricia Bauer CDS 1994 Sep 21 Francesco Ferraro <ferraro@bo.astro.it> J_A+AS_84_59.xml Walraven photometry of nearby southern OB associations J/A+AS/85/915 J/A+AS/85/915 Walraven Photometry of southern OB associations Walraven photometry of nearby southern OB associations E J De Geus J Lub E Van De Grift Astron. Astrophys. Suppl. Ser. 85 915 1990 1990A&AS...85..915D Clusters, open Photometry, VBLUW open clusters and associations: general photometry stars: colors Homogeneous Walraven (VBLUW) photometry is presented for 5260 stars in the region of five nearby southern OB associations: Sco-Cen (Sco OB2), Ori OB1, CMa OB1, Mon OB1, and Sct OB2. Note that the tables have been prepared at Lausanne/Geneve Observatory (star names in Lausanne/Geneva system, coordinates absent) For details about the Walraven photometric system, see <GCPD/11>
Walraven photometry (This file corresponds to a part of the tables III to XIX) Name Catalogue number number=1 the catalog abbreviations are: HD: Henry-Draper catalogue, CD: Cordoba Durchmusterung, CPD: Cape Photographic Durchmusterung, BD: Bonner Durchmusterung, AG: Astronomische Gesellschaft Katalog. --- m_Name Multuplicity index on star number=2 These indications are not in the published tables 1,2: components in a multiple system V: added to the name indicates possible variability D: added to the name indicates double star --- V log (intensity) in the Walraven V-band mag V-B V-B Walraven colour mag B-U B-U Walraven colour mag U-W U-W Walraven colour mag B-L B-L Walraven colour mag N Number of measurements --- Patricia Bauer CDS 1994 May 16 J_A+AS_85_915.xml The RATAN-600 7.6 cm catalog of radio sources from "Experiment Cold-80". J/A+AS/87/1 J/A+AS/87/1 RATAN-600 7.6 cm catalog of radio sources The RATAN-600 7.6 cm catalog of radio sources from "Experiment Cold-80". Yu N Parijskij N N Bursov N M Lipovka N S Soboleva A V Temirova Astron. Astrophys. Suppl. Ser. 87 1 1991 1991A&AS...87....1P VIII/33 : Spectral characteristics of RATAN Catalog (Bursov et al., =1989SoSAO..63...50B) J/A+AS/106/119 : Larionov et al., 1994, "A 3.9 GHz survey for declination -1 to 0deg" Radio sources catalogs radio sources: general radio sources: spectra A catalog containing 840 radio sources obtained during the Experiment Cold-80 at 7.6 cm wavelength using RATAN-600 are presented. The completeness of the list in the central zone is about 0.7-0.8 for sources with flux density 7.5-15 mJy. For sources brighter than 15 mJy the completeness reaches one. The number of sources-flux density differential curve is constructed.
The catalogue Name Name of Source: RC, J2000-based position; "t" stands for "twin" objects --- RAh right ascension (2000) h RAm right ascension (2000) min RAs right ascension (2000) s DE- declination sign --- DEd declination (2000) deg DEm declination (2000) arcmin DEs declination (2000) arcsec RAh1950 right ascension (1950) h RAm1950 right ascension (1950) min RAs1950 right ascension (1950) s e_RAs rms error on RA s DEd1950 declination (1950) deg DEm1950 declination (1950) arcmin DEs1950 declination (1950) arcsec e_DEs rms error on DE arcsec l_S7.6 Limit flag (>) on S7.6 --- S7.6 Flux density at wavelength of 7.6cm (3.95GHz) mJy e_S7.6 Flux density error in percent % S31 Flux density at wavelength of 31cm (0.97GHz) mJy e_S31 Flux density error in percent % Delta_h The deviation in elevation (Delta h) of the source position from the electrical axis of radio telescope in arcmin. arcmin Rem Remarks number=1 Sources marked with "D" were identified with objects of the 365 MHz (delta= 5deg +/-2deg) survey made at the University of Texas Radio Astronomy Observatory. Sources marked by "i" were identified by us with catalogued optical objects (galaxies, quasars, clusters of galaxies). Sources marked by "VLA" were observed with the Very Large Array The position and/or flux density of sources marked with asterisks may have larger errors than those shown. --- l_SpInd '<' for lower limit of SpInd, 'C' for curved spectrum. --- SpInd Spectral index. (S prop.to. nu**(-SpInd)) --- Joseph Florsch CDS 1993 Jun 14 UNKNOWN UNKNOWN * The catalogue was received on diskette in January 1993 at CDS; it was documented by Joseph Florsch [CDS] in June 1993. * The documentation was standardized in December 1995 J_A+AS_87_1.xml Compact radio sources in the galactic plane near l=140deg, b=0deg J/A+AS/88/355 J/A+AS/88/355 Compact radio sources in the galactic plane near l=1 Compact radio sources in the galactic plane near l=140deg, b=0deg D A Green Astron. Astrophys. Suppl. Ser. 88 355 1991 1991A&AS...88..355G radio sources: general surveys This paper presents a follow-up study of a flux density limited sample of 102 compact radio sources observed in the first DRAO Galactic plane survey (Green, 1989). These sources each have at least 250 mJy at 408 MHz and, although they are in a field centered at l = 140 deg, b = 0 deg, almost all of them are extragalactic. The multifrequency radio-spectral properties of these sources are presented, generally from observations at 151, 408, and 4850 MHz; some associations with the IRAS point sources are also discussed.
26P sources with at least 250 mJy at 408 MHz Some other 26P sources Source Source name --- n_Source note for source 26P1 number=1 26P1 has more that 250 mJy at 408 MHz, but is further than 4.0 deg from the center of the survey, so is excluded from the flux density limited sample of table1 --- S38MHz Flux density at 38 MHz mJy l_S151MHz limit flag on S151MHz --- S151MHz Flux density at 151 MHz mJy S408MHz Flux density at 408 MHz mJy l_S2695MHz limit flag on S2695MHz --- S2695MHz Flux density at 2695 MHz mJy S4760MHz Flux density at 4760 MHz mJy l_S4850MHz limit flag on S4850MHz --- S4850MHz Flux density at 4850 MHz mJy l_alpha(low) limit flag on alpha(low) --- alpha(low) spectral index between 408 and 151 MHz --- l_alpha(high) limit flag on alpha(high) --- alpha(high) spectral index between 408 and 4850 MHz --- n_alpha(high) note for alpha(high) number=2 When a, alpha high is the spectral index between 408 and 2695 MHz When b, alpha high is the spectral index between 408 and 4760 MHz --- James Marcout, Patricia Bauer CDS 1994 May 09 Dave Green J_A+AS_88_355.xml Optical positions of 221 radio stars obtained with the Bordeaux automatic meridian circle. J/A+AS/89/311 J/A+AS/89/311 Optical positions of 221 radio stars Optical positions of 221 radio stars obtained with the Bordeaux automatic meridian circle. Y Requieme J M Mazurier Astron. Astrophys. Suppl. Ser. 89 311 1991 1991A&AS...89..311R J/A+A/312/1031 : Positions + proper motions of radio stars ; (Argyle+, 1996) J/A+AS/105/429 : Optical position of radio stars (Carrasco+ 1994) Carlsberg Meridian Catalogue La Palma Number 4 1989, "Observations of positions of stars and planets: May 1984 to February 1988", Copenhagen University Observatory, Royal Greenwich Observatory, Real Instituto y Observatorio de La Armada en San Fernando. (Cat.<I/147>) Fricke, W., Schwan, H., Lederle, T. et al. 1988, Fifth Fundamental Catalogue (FK5), Part 1, Veroffentl. Aston. Rechen-Inst. Heidelberg, Number 32. (Cat.<I/149A>) Meridian observations Stars, radio meridian astrometry stars: radio This catalog contains optical positions of 221 radio stars observed with the Bordeaux automatic meridian circle. The observations were strictly differential, a convenient number of FK5 stars being used each night to calculate the instrumental parameters. The mean positions were corrected for chromatic refraction and also for photocenter effect in the case of duplicity. The asymptotic accuracy is expected to be about 0.05" for the Northern stars with a number of observations greater than 25. Some positions have been published previously, and the improved positions given here supersede earlier published data.
Optical Positions of 221 Radio Stars DM DM or FK5 number of the source number=1 These columns give the DM or FK5 number of the source (if any) and an alternative name. --- Oname Other identifier number=1 These columns give the DM or FK5 number of the source (if any) and an alternative name. --- m_Oname Component, if duplicity number=2 This column is flagged with a letter identifying the component (if there is more than one) of the star whose position is given. --- Vmag Observed mean visual magnitude number=3 The Vmag column gives the observed mean visual magnitude of the radio star. The f_Vmag column is flagged with a 'v' if the star is variable. For variable stars, the given magnitude corresponds to the maximum of light during the period of observation. --- f_Vmag Flagged if the star is variable number=3 The Vmag column gives the observed mean visual magnitude of the radio star. The f_Vmag column is flagged with a 'v' if the star is variable. For variable stars, the given magnitude corresponds to the maximum of light during the period of observation. --- pmRA Centennial proper motion in RA number=4 The pmRA and pmDE columns give the centennial proper motions in sec/century and arcsec/century respectively. Proper motions are taken from different astrometric catalogs. For a FK5 star, the given value originates in the FK5 catalog (Fricke et al. 1988, Cat.<I/149>). An asterisk in the f_pmRA or the f_pmDEC column indicates that the proper motion is taken from the Carlsberg meridian catalog Number 4 (1989, Cat.<I/147>). The values in pmRA and pmDEC are listed as zero if the proper motions are not known. s/ha f_pmRA Flagged if proper motion is from Carlsberg catalog number=4 The pmRA and pmDE columns give the centennial proper motions in sec/century and arcsec/century respectively. Proper motions are taken from different astrometric catalogs. For a FK5 star, the given value originates in the FK5 catalog (Fricke et al. 1988, Cat.<I/149>). An asterisk in the f_pmRA or the f_pmDEC column indicates that the proper motion is taken from the Carlsberg meridian catalog Number 4 (1989, Cat.<I/147>). The values in pmRA and pmDEC are listed as zero if the proper motions are not known. --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s f_RAs Flagged if correction of photocenter was applied --- o_RAs Number of observations in RA number=5 These columns give the number of observations in right ascension and declination, respectively. --- EpRAs Mean epoch of observations in RA number=6 These columns give the mean epoch of observations in right ascension and declination, respectively. Epochs are given as decimal years (- 1900), such as 87.93. yr pmDE Centennial proper motion in declination number=4 The pmRA and pmDE columns give the centennial proper motions in sec/century and arcsec/century respectively. Proper motions are taken from different astrometric catalogs. For a FK5 star, the given value originates in the FK5 catalog (Fricke et al. 1988, Cat.<I/149>). An asterisk in the f_pmRA or the f_pmDEC column indicates that the proper motion is taken from the Carlsberg meridian catalog Number 4 (1989, Cat.<I/147>). The values in pmRA and pmDEC are listed as zero if the proper motions are not known. arcsec/ha f_pmDE Flagged if proper motion is from Carlsberg catalog number=4 The pmRA and pmDE columns give the centennial proper motions in sec/century and arcsec/century respectively. Proper motions are taken from different astrometric catalogs. For a FK5 star, the given value originates in the FK5 catalog (Fricke et al. 1988, Cat.<I/149>). An asterisk in the f_pmRA or the f_pmDEC column indicates that the proper motion is taken from the Carlsberg meridian catalog Number 4 (1989, Cat.<I/147>). The values in pmRA and pmDEC are listed as zero if the proper motions are not known. --- DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec f_DEs Flagged if correction of photocenter was applied --- o_DEs Number of observations in Dec number=5 These columns give the number of observations in right ascension and declination, respectively. --- EpDEs Mean epoch of observations in Dec number=6 These columns give the mean epoch of observations in right ascension and declination, respectively. Epochs are given as decimal years (- 1900), such as 87.93. yr e_RAs Standard error in RA number=7 These columns give the positional errors in arcsec for right ascension and declination, respectively. Errors on the southern stars are somewhat larger, particularly the declination error. arcsec e_DEs Standard error in Dec number=7 These columns give the positional errors in arcsec for right ascension and declination, respectively. Errors on the southern stars are somewhat larger, particularly the declination error. arcsec Patricio Ortiz CDS 1999 Mar 30 UNKNOWN UNKNOWN "The catalogue was originally archived as A040 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_A+AS_89_311.xml 1612 MHz OH survey of IRAS point sources I. Observations made at Dwingeloo, Effelsberg and Parkes J/A+AS/90/327 J/A+AS/90/327 1612MHz OH survey of IRAS point sources 1612 MHz OH survey of IRAS point sources I. Observations made at Dwingeloo, Effelsberg and Parkes P te Lintel Hekkert J L Caswell H J Habing R F Haynes R P Norris Astron. Astrophys. Suppl. Ser. 90 327 1991 1991A&AS...90..327T II/125 : The IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) Masers Radio lines Stars, masers OH maser stars: OH/IR 2703 sources have been observed at the 1612MHz transition of OH, and 783 OH/IR stars were detected; 597 of these detections are new discoveries. The IRAS sources were detected on the basis of their IRAS fluxes at 12, 25 and 60um. The survey is 70% complete for IRAS sources in the Southern hemisphere (Dec<-10{deg}) with F(12um)>3Jy, with IR colors log(F25/F12)>-0.2 and log(F60/F12)<0.6 Note that the file catalog.dat contains all observed sources, with a flag indicating the detection or non-detection; the detected sources only are listed in the printed version of Table2, while sources without detectable 1612MHz emission are listed in Table3 (on microfiche)
Observations results (tables 2 and 3) IRAS IRAS name --- OH-Name OH name --- Dflag Detection flag number=1 The detection flag is 1 = non-detection 2 = likely detection 3 = standard profile --- Peaks Number of peaks in spectrum --- GLON Galactic longitude deg GLAT Galactic latitude deg VL Lower velocity (blue shifted pike) number=2 for single-peak detections, the values are in VL and SL, (VH and SH are set to 0) km/s VH Higher velocity (red shifted pike) number=2 for single-peak detections, the values are in VL and SL, (VH and SH are set to 0) km/s SL 1612MHz Flux density at VL number=2 for single-peak detections, the values are in VL and SL, (VH and SH are set to 0) Jy SH 1612MHz Flux density at VH number=2 for single-peak detections, the values are in VL and SL, (VH and SH are set to 0) Jy F25 25-micron IRAS flux Jy R21 log(F(25)/F(12)) ratio of IRAS fluxes --- R32 log(F(60)/F(25)) ratio of IRAS fluxes --- VAR Variability probability from IRAS --- LRS Number of IRAS Low Resolution Spectra --- Francois Ochsenbein CDS 1992, 15-Apr-1998 Dec 18 UNKNOWN UNKNOWN * December 1992: the electronic version of the table was e-mailed to CDS by Hekkert te Lintel. * April 1998: Non-measured sources without OH-Name were removed. The documentation (this ReadMe file) was revised and completed. J_A+AS_90_327.xml A photometric study of the bright cloud B in Sagittarius. VII. 1165 new variable stars and 65 diffuse objects. J/A+AS/90/451 J/A+AS/90/451 Variables and Nebulae in Sgr B A photometric study of the bright cloud B in Sagittarius. VII. 1165 new variable stars and 65 diffuse objects. A Terzan E Gosset Astron. Astrophys. Suppl. Ser. 90 451-493 1991 1991A&AS...90..451T J/A+AS/49/715 : (621 variables) J/A+AS/76/205 : (1592 variables and 30 diffuse objects) Galaxy: structure long-period variables A field in the Sagittarian bright cloud in the direction of the Galactic center is investigated by means of the B, V, and R Schmidt plates at the ESO, and 1165 variable stars are reported. The position, R magnitudes, epochs, and amplitudes of variation are given for each star, and the surface density per square degree of variable stars increases from 1.7 to 65. The number of variables in the present field is similar to that for field A, and variables of type L and/or M are more densely numerous toward the center of the Galaxy than at other locations. Of the objects listed, 65 are given with potential classifications based on morphological data from the B and R Schmidt plates. The preliminary observations suggest a success rate of 42 percent on the precise prediction of the object types.
Variables in Sgr B cloud TerzV Runnning Number --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg l_Rmax '<' when Rmax is an upper value --- Rmax Red magnitude at Maximum mag u_Rmax ':' for inaccurate R(max) value. --- r_Rmax Index of plate in table 1 --- l_Rmin '>' when R(min) is a lower value --- Rmin Red magnitude at minimum mag u_Rmin ':' for inaccurate R(min) value. --- r_Rmin Index of plate in table 1 --- A Observed magnitude amplitude mag Remarks Other names and Remarks: B or V indicate a brightness variation on the B and/or V plates Other remarks: see the paper --- Francois Ochsenbein CDS 1995 Jul 07 UNKNOWN UNKNOWN * 27-Oct-1992: Catalogue provided by Eric Gosset, and first archived * 07-Jul-1995: reformatted to be compatible with other parts J/A+AS/49/715 and J/A+AS/76/205 J_A+AS_90_451.xml New proper-motion stars south of declination -40deg and right ascension between 04h30 and 16h00 J/A+AS/91/129 J/A+AS/91/129 New proper-motion stars Dec<-40, 4h30<RA<16h New proper-motion stars south of declination -40deg and right ascension between 04h30 and 16h00 H Wroblewski C Torres Astron. Astrophys. Suppl. Ser. 91 129 1991 1991A&AS...91..129W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/78/231 : Dec<-40, 0<RA<4h30, stars 1 to 144 (Wroblewski+ 1989) J/A+AS/105/179 : Dec<-40, 16<RA<24h, stars 522 to 1069 (Wroblewski+ 1994) J/A+AS/115/481 : -30<Dec<-5, 0<RA<9h, stars 1070 to 1563 (Wroblewski+ 1996) J/A+AS/83/317 : LTT stars, Dec<-40, 0<RA<4h30 (Wroblewski+ 1990) J/A+AS/92/449 : LTT stars, Dec<-40, 4h30<RA<16h (Wroblewski+ 1992) J/A+AS/110/27 : LTT stars, Dec<-40, 16<RA<24h (Wroblewski+, 1995) Wroblewski H., Torres C.: 1989, A&AS 78, 231 Proper motions astrometry proper motions Data are given for 377 new proper-motion stars with {mu}>=0.15arcsec/yr. The stars 1 to 144 are given in Wroblewski and Torres (1989),
The catalogue WT Running number --- Loc Localisation (area and number) --- mpg Photographic magnitude, accurate to 0.5mag mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RAh2000 Right Ascension 2000 (hours) h RAm2000 Right Ascension 2000 (minutes) min RAs2000 Right Ascension 2000 (seconds) s DE-2000 Declination 2000 (sign) --- DEd2000 Declination 2000 (degrees) deg DEm2000 Declination 2000 (minutes) arcmin DEs2000 Declination 2000 (seconds) arcsec pm Total proper motion arcsec/yr e_pm Mean error on pm arcsec/yr pmPA Position angle (North to East) of the proper motion in J2000 equinox deg Remark Remarks number=1 '4' when proper-motion is the mean of #4 pairs of plates (*), '6' when proper-motion is the mean of #6 pairs (**). --- James Marcout, Francois Ochsenbein CDS 1994 Feb 22 UNKNOWN UNKNOWN Keypunched at CDS in February 1994 The number 259 at 12 47 20.3 -41 43 02 was changed in 359 J_A+AS_91_129.xml Catalogue of blue stars between the Magellanic Clouds J/A+AS/91/171 J/A+AS/91/171 Catalogue of blue stars between the Magellanic Catalogue of blue stars between the Magellanic Clouds S Demers M J Irwin Astron. Astrophys. Suppl. Ser. 91 171 1991 1991A&AS...91..171D Magellanic Clouds A list of 1679 blue stars located in a region of the southern sky between the Magellanic Clouds is presented. Equatorial coordinates and photographic V and B - V are given for stars brighter than V = 18.5. The instrumental magnitudes obtained from UKST IIIa-J and IIIa-F plates are calibrated with nearly 200 stars with CCD B and V observations. This list can be used for follow-up identification, spatial distribution, and other studies of young OB stars belonging to the Magellanic Clouds.
Blue stars between MC Id Running number --- RAH Right Ascension 1950 h RAM Right Ascension 1950 min RAS Right Ascension 1950 s DE- Declination 1950 (sign) --- DED Declination 1950 deg DEM Declination 1950 arcmin DES Declination 1950 arcsec V V magnitude mag B-V Color index mag Francois Ochsenbein CDS 1993 Jan 04 J_A+AS_91_171.xml A list of steep spectrum radio spectra sources J/A+AS/91/337 J/A+AS/91/337 A list of steep spectrum radio spectra sources A list of steep spectrum radio spectra sources N S Soboleva A V Temirova P Reich. Astron. Astrophys. Suppl. Ser. 91 337 1991 1991A&AS...91..337S radio sources: general radio sources: spectra A comparison of three high-sensitivity catalogs of radio sources at meter and centimeter wavelengths, UTRAO (365 MHz), GB (4.85 GHz) and RC (3.94 GHz), has been made. As a result of this comparison the spectral index distribution for about 2000 UTRAO-GB objects in the declination strip of 5 +/-2 deg was computed and a list of about 300 radio sources with a steep spectrum (alpha is greater than 1.1, S varies as nu exp alpha) was obtained. It is shown that the spectral index distributions of unresolved and double radio sources differ. The mean spectral indices for these two classes of objects also differ. A systematic shift in the coordinates between the catalogs (UTRAO-GB) was estimated to be about +1.2 s in right ascension and -14 arcsec in declination.
A list of steep spectrum radio sources alpha Spectral index (S proportional to nu^(-alpha)) --- RAh right ascension (1950) h RAm right ascension (1950) min RAs right ascension (1950) s DEd declination (1950) deg DEm declination (1950) arcmin DEs declination (1950) arcsec Rem Source parameters from the Texas radio source catalogue (Douglas et al. 1980, Univ.Texas., Publ. 17) P: point source D: double source AD: asymetrical double strings like -1+1 refer to possible lobe shifts in the Texas catalogue --- Joseph Florsch CDS 1993 Jun 14 J_A+AS_91_337.xml An Extragalactic Database. IV. Errors and misprints in catalogues of galaxies. J/A+AS/91/371 J/A+AS/91/371 An Extragalactic Database. IV.Errors and misprints An Extragalactic Database. IV. Errors and misprints in catalogues of galaxies. G Paturel C Petit N Kogoshvili P Dubois L Bottinelli P Fouque R Garnier L Gouguenheim Astron. Astrophys. Suppl. Ser. 91 371 1991 1991A&AS...91..371P galaxies: general *** No Description Available ***
NGC/IC with several names Errors in MCG etc... Errors in PGC NAME Name of the galaxy as appearing in the original catalogue --- RA Right ascension for 1950 in table1 & table2, for 2000 in table3 HMS DE Declination for 1950 in table1 & table2, for 2000 in table3 DMS code describing the kind of error: =1 error in coordinates =2 error in name =3 missing name =4 miscellaneous =5 not a galaxy, or merged with another galaxy --- Comments Complete explanation of the error -- Francois Ochsenbein CDS 1993 Jan 04 J_A+AS_91_371.xml Secondary Spectrophotometric standards J/A+AS/92/1 J/A+AS/92/1 Secondary Spectrophotometric standards Secondary Spectrophotometric standards I N Glushneva A V Kharitonov L N Knyazeva V I Shenavrin Astron. Astrophys. Suppl. Ser. 92 1 1992 1992A&AS...92....1G III/126 : Stellar Spectrophotometric Catalogue (Burnashev, 1985) III/202 : Spectrophotometric Catalogue of Stars (Kharitonov+, 1988) III/207 : Moscow Spectrophotometric Catalog (Glushneva+ 1998) III/208 : Sternberg Spectrophotometric Catalog (Glushneva+ 1998) III/209 : Spectrophotometric Standards (Biryukov+ 1998) Stars, normal Spectrophotometry spectrophotometry catalogues stars: general Energy distribution data on 238 secondary standard stars in the range 3200-7600{AA} with a 50{AA} step are presented. These stars are common to the Catalogue of the Sternbergh State Astronomical Institute and to the Fessenkov Astrophysical Institute (Alma-Ata). For these stars, the differences between the two catalogues do not exceed 5%, and the mean internal accuracy of both catalogue data in this wavelength range are about 3.5%. For 99 stars, the energy distribution in the near infra-red (6000-10800{AA}) are also presented.
Summary of stars with SIMBAD data (table2) HR HR number (Bright Star), See Cat. <V/50> --- m_HR Multiplicity (/ followed by last digit) --- FlagIR when star also observed in near-IR (table5) --- RAh Right Ascension J2000 (hours) number=1 Data are from SIMBAD h RAm Right Ascension J2000 (minutes) number=1 Data are from SIMBAD min RAs Right Ascension J2000 (seconds) number=1 Data are from SIMBAD s DE- Declination J2000 (sign) number=1 Data are from SIMBAD --- DEd Declination J2000 (degrees) number=1 Data are from SIMBAD deg DEm Declination J2000 (minutes) number=1 Data are from SIMBAD arcmin DEs Declination J2000 (seconds) number=1 Data are from SIMBAD arcsec Bmag Blue magnitude number=1 Data are from SIMBAD mag Vmag Visual magnitude number=1 Data are from SIMBAD mag SpType Spectral type number=1 Data are from SIMBAD --- Standard stars Seq Running number --- --- text --- HR Number in Bright Star catalogue (Cat. <V/50>) --- --- text --- HD Number in HD catalogue (Cat. <III/135>) --- Name Name of star --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin Vmag Magnitude mag B-V Color index mag U-B Color index mag SpType Spectral type and luminosity class --- E Energy distribution in 10^-4^erg/(cm^2^.s.cm) in range 3225-7525{AA} with a step of 50{AA} 10-7W/m2/cm Optical wavelength range 322.5-767.5nm HR Number in Bright Star catalogue (Cat. <V/50>) --- E Energy distribution data in erg/(cm**2 s cm) in range 3225-7675{AA}, with a step of 50{AA} mW/m2/cm Near-IR wavelength range 597.5-1082.5nm HR Number in Bright Star catalogue (Cat. <V/50>) --- E Energy distribution data in erg/(cm**2 s cm) in range 5875-10875{AA}, with a step of 50{AA} mW/m2/cm Veta Avedisova INASAN Francois Ochsenbein CDS 1998 Dec 18 UNKNOWN UNKNOWN * 13-Mar-1993: first version received from the A&A Editor (no table1) * 18-Dec-1998: energy distribution of the standard stars (table1) supplied by Veta Avedisova. The table "stars.dat" was added at CDS to supply minimal data (extracted from SIMBAD) about the studied stars. J_A+AS_92_1.xml OH/IR stars close to the Galactic centre. I. Observational data J/A+AS/92/43 J/A+AS/92/43 OH/IR stars close to the Galactic centre. I. Obs OH/IR stars close to the Galactic centre. I. Observational data M Lindqvist A Winnberg H J Habing H E Matthews Astron. Astrophys. Suppl. Ser. 92 43 1992 1992A&AS...92...43L Galaxy: center stars: circumstellar matter stars: OH/IR *** No Description Available ***
OH/IR stars close to Galactic centre Number Number --- Source OH name (galactic longitude & latitude) --- RA1950H Right ascension for 1950 h RA1950M Right ascension for 1950 min RA1950S Right ascension for 1950 s bracket ( --- RA-rms rms error of RA1950 s bracket ) --- DE1950- Declination 1950 sign --- DE1950D Declination 1950 deg DE1950D Declination 1950 arcmin DE1950D Declination 1950 arcsec bracket ( --- DE-rms rms error of DE1950 arcsec bracket ) --- VH Radial velocity (LSR) of the high-velocity component km/s SH Peak flux density of the high-velocity component Jy IH Integrated 1612 MHz flux density of the high-velocity component Jy.km/s VL Radial velocity (LSR) of the low-velocity component km/s SL Peak flux density of the low-velocity component Jy IL Integrated 1612 MHz flux density of the low-velocity component Jy.km/s C Correction factor due to the primary beam attenuation --- Vexp Expansion velocity of the shell =(VH-VL)/2 km/s Vc Radial velocity (LSR) of the star = (VH+VL)/2 km/s Date Date of observation YYMMDD Remarks Comments on individual spectra: H = Habing et al., 1983, A&A 128, 320 W = Winnberg et al., 1985, ApJ 291, L45 R = Spectrum smoothed O = Only one velocity component V = Velocity from Habing et al., 1983 --- Francois Ochsenbein CDS 1993 Jan 04 J_A+AS_92_43.xml New proper motion determination of Lyuten catalogue stars (LTT) south of declination -40 and right ascension between 04h30 and 16h00m J/A+AS/92/449 J/A+AS/92/449 Proper-motion of LTT stars New proper motion determination of Lyuten catalogue stars (LTT) south of declination -40 and right ascension between 04h30 and 16h00m H Wroblewski C Torres Astron. Astrophys. Suppl. Ser. 92 449 1992 1992A&AS...92..449W I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/78/231 : Dec<-40, 0<RA<4h30, stars 1 to 144 (Wroblewski+ 1989) J/A+AS/91/129 : Dec<-40, 0<RA<4h30, stars 145 to 521 (Wroblewski+ 1991) J/A+AS/105/179 : Dec<-40, 16<RA<24h, stars 522 to 1069 (Wroblewski+ 1994) J/A+AS/115/481 : -30<Dec<-5, 0<RA<9h, stars 1070 to 1563 (Wroblewski+ 1996) J/A+AS/83/317 : LTT stars, Dec<-40, 0<RA<4h30 (Wroblewski+ 1990) J/A+AS/110/27 : LTT stars, Dec<-40, 16<RA<24h (Wroblewski+, 1995) Luyten W.J. 1957, A Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motions Exceeding 0.2 arcsec Annualy (The Lund Press, Minneapolis, Minnesota). Luyten W.J. 1979, LHS Catalogue, University of Minnesota, Minneapolis, Minnesota. (Cat. <I/87>) Proper motions astrometry proper motions Data are given for 205 LTT stars found on 23 areas, covering 25 square degrees each, south of declination -40D and right ascension between 04h 30m and 16h 00m. Four stars present differences in proper motion >=0.10", three present differences in position angle >20deg and one presents those differences in both values.
Positions and relative proper motions Seq Running number --- LTT Star number in Luyten's catalogue --- Loc Localisation (area and number) --- mpg Photographic magnitude, accurate to 0.5mag mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RAh2000 Right Ascension 2000 (hours) h RAm2000 Right Ascension 2000 (minutes) min RAs2000 Right Ascension 2000 (seconds) s DE-2000 Declination 2000 (sign) --- DEd2000 Declination 2000 (degrees) deg DEm2000 Declination 2000 (minutes) arcmin DEs2000 Declination 2000 (seconds) arcsec pm Total proper motion arcsec/yr e_pm Mean error on pm arcsec/yr pmPA Position angle (North to East) of the proper motion in J2000 equinox deg Dpm Difference LTT pm minus pm (this work) number=1 It can be seen that most proper motions given in LTT are larger than those determined by us. It is important to point out that stars 3 (LTT 2073), 22 (LTT 2681), 59 (LTT 3536), 179 (LTT 5731) and 196 (LTT 6127) show considerable differences (>0.10") arcsec Remarks Remarks number=2 '4' when proper-motion is the mean of 4 pairs of plates. '6' when proper-motion is the mean of 6 pairs of plates. '1' when LTT and present PA value differ by 20deg or more. Stars 6 (LTT 2214), 36 (LTT 2810), 151 (LTT 5365) and 179 (LTT 5731) differ by 20deg or more. The case of star 151 (LTT 5365) is remarkable because Lyuten estimates for it a position angle of 261deg, while our result is 1.6deg. '2' The star 90 (LTT 3915) was not found in the position given by Luyten's Catalog but almost one degree south. The star LTT 5582 was not found in our plates. --- James Marcout, Patricia Bauer CDS 1997 Mar 13 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_92_449.xml Intensive Photometry of southern Be variables. II Summer objects J/A+AS/92/533 J/A+AS/92/533 Southern Summer Be Variables-Photometry Intensive Photometry of southern Be variables. II Summer objects L A Balona J Cuypers F Marang Astron. & Astrophy. Supp. 92 533 1992 1992A&AS...92..533B Stars, Be Stars, variable This paper presents further data from an intensive photometric campaign on some bright southern Be stars to search for periodic light variations.
b magnitudes for NV Pup b magnitudes for NW Pup b magnitudes for 19 Mon b magnitudes for 27 CMa b magnitudes for 28 CMa b magnitudes for 39 Cru b magnitudes for 48 Lib b magnitudes for Alp Ara b magnitudes for Alp Eri b magnitudes for Chi Oph b magnitudes for DU Eri b magnitudes for DX Eri b magnitudes for Del Cen b magnitudes for Eps Cap b magnitudes for Eta Cen b magnitudes for FT CMa b magnitudes for FV CMa b magnitudes for HD137518 b magnitudes for HD91188 b magnitudes for HP CMa b magnitudes for HR3135 b magnitudes for HR4221 b magnitudes for HR4618 b magnitudes for HR8408 b magnitudes for IU Vel b magnitudes for Iot Ara b magnitudes for Kap1 Aps b magnitudes for Kap CMa b magnitudes for Lam Cru b magnitudes for Lam Eri b magnitudes for Mu Cen b magnitudes for Mu Pic b magnitudes for Ome Ori V magnitudes for Omi Aqr b magnitudes for Omi Aqr b magnitudes for Psi2A qr b magnitudes forZet Oph JD Julian date of observation d b Stromgren b magnitude mag B magnitudes for NGC3766-151 B magnitudes for NGC3766-15 B magnitudes for NGC3766-1 B magnitudes for NGC3766-239 B magnitudes for NGC3766-240 B magnitudes for NGC3766-264 B magnitudes for NGC3766-26 B magnitudes for NGC3766-27 B magnitudes for NGC3766-291 B magnitudes for NGC3766-301 B magnitudes for NGC3766-53 B magnitudes for NGC3766-63 B magnitudes for NGC3766-81 B magnitudes for NGC3766-88 JD Julian date of observation d B Johnson B magnitude mag V mag. and Johnson V-B for NGC3766-15 V mag. and Johnson V-B for NGC3766-1 V mag. and Johnson V-B NGC3766-88 JD Julian date of observation d V Johnson V magnitude mag B-V Johnson B-V color mag U-B Johnson U-B color mag B mag. and Johnson V-B NGC3766-63 JD Julian date of observation d B Johnson B magnitude mag B-V Johnson B-V color mag U-B Johnson U-B color mag V mag. and Stromgren colors for 27 CMa V mag. and Stromgren colors for 28 CMa V mag. and Stromgren colors for 48 Lib V mag. and Stromgren colors for Alp Ara V mag. and Stromgren colors for Chi Oph V mag. and Stromgren colors for DU Eri V mag. and Stromgren colors for DX Eri V mag. and Stromgren colors for Eps Cap V mag. and Stromgren colors for Eta Cen V mag. and Stromgren colors for HD137518 V mag. and Stromgren colors for HR8408 V mag. and Stromgren colors for Kap1 Aps V mag. and Stromgren colors for Mu Cen V mag. and Stromgren colors Ome Ori V magnitudes for Omi Aqr V mag. and Strom. colors Psi2 Aqr V mag. and Stromgren colors Zet Oph JD Julian date of observation d V Johnson V magnitude mag b-y Stromgren b-y color mag m1 Stromgren m1 mag c1 Stromgren c1 mag details of file contents id File name --- name Star name --- alt HR or CPD number --- HD HD --- HDno HD number --- spec Spectral Type --- note --- mag_c Color for magnitude measures --- col1 First color, if any --- col2 Second color, if any --- c1 third color, if present --- rem Remarks (variable or period) --- Nancy G. Roman ADC/SSDOO 1995 Jul 07 J_A+AS_92_533.xml The interstellar medium of M 31. III. Narrow-band imagery in H-alpha and SII. J/A+AS/92/625 J/A+AS/92/625 Interstellar medium of M 31. III. Narrow-band The interstellar medium of M 31. III. Narrow-band imagery in H-alpha and SII. R A M Walterbos R Braun Astron. Astrophys. Suppl. Ser. 92 625 1992 1992A&AS...92..625W galaxies: individual (M 31) galaxies: spiral HII regions planetary nebulae: general supernova remnants Deep CCD imagery in H alpha and (SII) is presented of the major spiral arms of M31 with particular attention given to the data reduction and the analysis of the (SII)/H alpha flux ratios. A diffuse ionized gas noted in the images is analyzed which shows higher (SII)/H alpha ratios, and 967 discrete nebulae are listed with gray-scale images, finding charts, and absolute fluxes. The differential H-alpha luminosity function is found to have a slope of -0.95 for brighter objects and flattens out below a critical level. The curve is shown to correspond to the point at which single-star ionization accounts for the H alpha luminosities and is consistent with previous observations. The catalog of objects and fluxes is the largest existing sample of this type, and the unresolved objects in the sample are considered to be planetary nebulae.
Catalog of ionized nebulae in M31 ID Source ID in the catalog. --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s e_RA rms uncertainty on right ascension s DE- Declination sign --- DEd Declination 1950 deg DEm DEclination 1950 arcmin DEs Declination 1950 arcsec e_DE rms uncertainty on declination arcsec MajAxis Source major axis. Nominally unresolved sources have size 0.0 arcsec e_MajAxis rms uncertainty on source major axis or upper limit for the size of unresolved sources arcsec MinAxis Source minor axis. Nominally unresolved sources have size 0.0 arcsec e_MinAxis rms uncertainty on source minor axis or upper limit for the size of unresolved sources arcsec PA Major axis position angle (east of north) deg e_PA rms uncertainty on source minor axis position angle deg Rmin Minimum radius of the annular regions centered on the source number=1 Minimun and maximum radius of the annular regions centered on the source and contained within an isolating box which were used to determine the local background level and its uncertainty for extended sources in the catalog. Sources with R_{min} = R_{max} = 0 were fitted with an elliptical Gaussian. arcsec Rmax Maximum radius of the annular regions centered on the source number=1 Minimun and maximum radius of the annular regions centered on the source and contained within an isolating box which were used to determine the local background level and its uncertainty for extended sources in the catalog. Sources with R_{min} = R_{max} = 0 were fitted with an elliptical Gaussian. arcsec H-alp Integrated source flux in Halpha (10^-15^ erg/cm2/s) 10-18W/m2 e_H-alp rms uncertainty on Halpha flux 10-18W/m2 [SII] Integrated source flux in the [SII] 6717 and 6731 Angstrom lines (10^-15^ erg/cm2/s) Negative values correspond to 3 sigma upper limits. 10-18W/m2 e_[SII] rms uncertainty on [SII] flux 10-18W/m2 X Major axis coordinate of the source arcmin Y Minor axis coordinate of the source arcmin R1 Radius within the galaxy of the spiral arm "most likely" associated with the source number=2 The values are based on the kinematic model of Braun (1991). arcmin R2 Second possible radius number=2 The values are based on the kinematic model of Braun (1991). arcmin V1 Radial heliocentric velocity corresponding to the "most likely" radius R1 number=2 The values are based on the kinematic model of Braun (1991). km/s V2 Radial heliocentric velocity corresponding to R2 number=2 The values are based on the kinematic model of Braun (1991). km/s dY1 Minor axis offsets of the source position from the "most likely" spiral arm arcmin dY2 Minor axis offsets of the source position from the second arm arcmin tau1 Optical depth at Halpha along the source line-of-sight using a fixed Galactic foreground contribution and a variable contribution from dust in M31, assuming a source position at the middle of the "most likely" spiral arm at the radius R1 number=3 Optical depths are based on integrations of high resolution HI data (Braun 1990b) after correction for HI optical depth and calibrated with dust-to-gas ratios of Braun and Walterbos (1991). --- tau2 Like tau1 but at the radius R2 --- H-alp' Optical-depth-corrected flux in Halpha (10^-15^ erg/cm2/s) using the "most likely" optical depth from tau1 10-18W/m2 e_H-alp' rms uncertainty on H-alp' 10-18W/m2 [SII]' Optical-depth-corrected flux in [SII] 6717 and 6731 Angstrom line (10^-15^ erg/cm2/s) using the "most likely" optical depth tau1 10-81W/m2 e_[SII]' rms uncertainty on [SII]' 10-81W/m2 Xref Cross-reference ID to larger sources within the catalog in which the listed entry is embedded. --- Notes A lower case c means uncertain calibration, S? implies that the source coincides with a continuum source and may be a star, although this is by no means certain, since often the remaining Halpha signal is too strong to be due to the faint star that is visible in the red continuum. C1, C2, R1, R2, D1, and D2 indicate morphology, as described in the paper --- Patricia Bauer CDS 1994 Jun 10 Rene Walterbos <rwalterb@NMSU.Edu> J_A+AS_92_625.xml The spectrum of the VV Cep star KQ Puppis (Boss 1985). II. Atlas of the optical and ultraviolet spectrum J/A+AS/92/685 J/A+AS/92/685 Atlas of Optical and Ultraviolet Spectrum The spectrum of the VV Cep star KQ Puppis (Boss 1985). II. Atlas of the optical and ultraviolet spectrum A Altamore C Rossi R Viotti G B Baratta Astron. Astrophys. Suppl. Ser. 92 685-719 1992 1992A&AS...92..685A atlases binaries: spectroscopic spectrophotometry stars: emission-line, Be stars: individual (KQ Pup) ultraviolet: general An Atlas is presented of the high-resolution spectrum of the VV Cep M1-2Iab + Be variable KQ Pup (Boss 1985). The Atlas is based on UV observations obtained in 1979 with the IUE (covering the region from 1223 A to 3228 A) and on coude plates covering the blue to the optical UV. The equivalent widths and radial velocities of the main features present in the optical spectra are given. Additional CAT/CES observations of H-alpha are shown. The Atlas should be a basis for future investigation on luminous cool variables.
KQ Pup in Dec 1969 (Plate F68274) KQ Pup in Mar 1979 (Plate G10250) KQ Pup in Feb 1983 (Plate G12849) LAB-WL Laboratory wavelength (in A) of the transition. 0.1nm ION Ion designation --- MULT Moore's (1945) multiplet number of the main contributor. --- F "F" refers to a forbidden transition. --- ObsWL Heliocentric central wavelength of the measured spectral feature. For Plate F68274 the wavelength scale is determined by the M star lines. 0.1nm u_ObsWL uncertainty flag on ObsWL --- A/E Nature of the line: A=absorption, E=emission. --- W Total width (in A) of the measured features. 0.1nm u_W Uncertainty flag on W --- EW Equivalent width (in A). 0.1nm u_EW Uncertainty flag on EW --- FLINE Level of the continuum local to the feature (in 10-13 erg cm-2 s-1 A-1) corrected for an interstellar extinction of E(B-V)=0.14. 10-15W/m2/nm CONT Integrated emission line flux in 10-13 erg cm-2 s-1, corrected for the interstellar exctinction. 10-15W/m2/nm RV Heliocentric radial velocity in km s-1. In Plate F68274 the radial velocities are referred to that of the M star. km/s u_RV Uncertainty flag on RV --- REM Remarks: db = double structure of the line. ? = uncertain line. bl = blend of two or more lines. broad = broad line. VE = violet emission component. RE = red emission component. CA = central absorption.; M* = photometric absorption of the M star. i.s. = interstellar line. Eta Car = emission line present in the spectrum of Eta Carinae. sat = saturated line. --- Francois Ochsenbein CDS 1993 Feb 19 J_A+AS_92_685.xml uvby-beta observations of 528 type B stars with V between the 8th and 9th magnitude. J/A+AS/92/841 J/A+AS/92/841 uvby-beta observations of 528 B stars uvby-beta observations of 528 type B stars with V between the 8th and 9th magnitude. J Knude Astron. Astrophys. Suppl. Ser. 92 841-861 1992 1992A&AS...92..841K Photometry, uvby, beta Stars, B-type The paper presents uvby-beta measurements of 528 type B stars selected from the SAO Catalog on the basis of two criteria: the spectral types in the range B3-B5 and mV between the 8th and the 9th magnitude. Reddening independent (c1) values are estimated from the spectral classification and compared to the observed values. No systematic trend with observed (b-y), H-beta, or spectral type appears to be present, but the range of (c1) residuals is surprisingly large. A rather large part of the stars has small beta values, smaller than for the BIa supergiants. Only two are classified as O stars and most of them have the suffix e, ne, or nne. Most beta values for the O type stars are slightly above the upper limit of 2.585 m.
Photometric results SAO SAO Number --- HD HD Number --- DM Durchmusterung number --- Sp Spectral classification --- Vmag V magnitude mag b-y b-y index mag m1 m_1 index ((v-b) - (b-y)) mag c1 c_1 index ((u-v) - (v-b)) mag beta beta index mag Francois Ochsenbein CDS 1993 Mar 03 UNKNOWN UNKNOWN A few errors were corrected compared to the printed version: SAO 115686 replaced by SAO 114686 HD numbers corrected for the SAO numbers: 95199 95272 95653 95680 132876 132895 134219 151812 151931 152316 152318 152360 153113 161208 172183 227429 236941 241791 J_A+AS_92_841.xml Stromgren photometry of three double mode high amplitude Delta Scuti stars J/A+AS/93/189 J/A+AS/93/189 Stromgren photometry of three double mode high Stromgren photometry of three double mode high amplitude Delta Scuti stars E Rodriguez A Rolland P Lopez De Coca E Garcia-Lobo J L Sedano Astron. Astrophys. Suppl. Ser. 93 189 1992 1992A&AS...93..189R Photometry Stars, variable delta Scuti photometry stars: variables: general uvby-beta photoelectric photometric observations of the three double-mode high-amplitude Beta-Scuti stars AE UMa, RV Ari and BP Peg are presented. Periodogram analyses are performed using the Fourier Transform Method. In all three stars the power spectra are complex, and a large number of frequencies are identified. For each star, all these frequencies are shown to be harmonics or combinations of two main frequencies nu1 and nu2 corresponding to the fundamental and first radial pulsation modes, respectively. Intrinsic b - y, m1, and c1 values are derived and the physical parameters of these stars are determined.
Standard uvby (AE UMa - BD+44 1898) Standard uvby (RV Ari - HD 14107) Standard uvby (BP Peg - HD 205542) HJD Heliocentric Julian Day day Du Stroemgren filter magnitude difference mag Dv " mag Db " mag Dy " mag Standard Hbeta(AE UMa) Standard Hbeta(RV Ari) Standard Hbeta(BP Peg) HJD Heliocentric Julian Day day H-beta Standard Hbeta mag CDS 1993 Mar 19 J_A+AS_93_189.xml Astrometry of globular clusters. I. Relative proper motions for stars in 47 Tuc. J/A+AS/93/293 J/A+AS/93/293 Astrometry of globular clusters. I. Relative Astrometry of globular clusters. I. Relative proper motions for stars in 47 Tuc. H J Tucholke Astron. Astrophys. Suppl. Ser. 93 293 1992 1992A&AS...93..293T globular clusters: individual (47 Tuc) The study determines relative proper motions for stars brighter than 17.0 m in a 1.5 x 1.5 deg field centered on the globular cluster 47 Tuc (NGC 104). Proper motion and membership probabilities are tabulated for 3076 stars within 32 arcmin of the cluster center. A proper motion of 47 Tuc relative to the SMC is derived, which relies on the assumption that the mean proper motion of field stars is the same as that in the nearby field of NGC 362, and on the detection of SMC stars in that field. The resulting space motion confirms the membership of 47 Tuc in the rapidly rotating, flattened, metal-rich disk subgroup of the galactic cluster system. Relative proper motions for stars centered on the globular cluster NGC 362 are determined. NGC 362 is found to exhibit a highly eccentric orbit, typical for a member of the halo subgroup of the galactic globular cluster system. The perigalactic distance of NGC 362 is very small (less than about 1 kpc).
Stars within 45' of 47 Tuc centre N Running number --- Id Identifier: Prefix 3- or 5-: Hesser & Hartwick, 1977, ApJS 33, 361 (Figs 3 or 5) Prefix D or E: Chun & Freeman, 1978, AJ 83, 376 (rings D or E) No prefix: Lee, 1977, A&AS 27,381. --- B Magnitude in B (+/- 0.25 mag) mag u_B Uncertainty flag on B --- B-R Color index (+/- 0.40 mag) mag u_B-R Uncertainty flag on B-R --- x Relative position to adopted cluster centre (1 pixel = 0.7695 arcsec) pix y Relative position to adopted cluster centre (1 pixel = 0.7695 arcsec) pix mua Proper motion in RA (mu_alpha.cos(delta)) mas/a e_mua Error on mua mas/a mud Proper motion in Dec mas/a e_mud Error on mud mas/a N1 Number of first-epoch plates --- N2 Number of second-epoch plates --- Pr Membership probability % RAh Right Ascension 1950 (hours) (Epoch 1985.5, Perth-70-System, +/- 0.4") h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) (Epoch 1985.5, Perth-70-System, +/- 0.4") --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Francois Ochsenbein CDS 1993 Apr 09 J_A+AS_93_293.xml Astrometry of globular clusters. II. Relative proper motions and the space motion of NGC 362 J/A+AS/93/311 J/A+AS/93/311 Astrometry of globular clusters. II. Relative Astrometry of globular clusters. II. Relative proper motions and the space motion of NGC 362 H J Tucholke Astron. Astrophys. Suppl. Ser. 93 311 1992 1992A&AS...93..311T globular clusters: individual (NGC 362) *** No Description Available ***
NGC 362 stars N Running number --- Id Identifier: Prefix A: Alcaino, 1976, A&AS 26, 359 No prefix: Harris, 1982, ApJS 50, 573 --- B Magnitude in B (+/- 0.25 mag) mag u_B Uncertainty flag on B --- B-R Color index (+/- 0.40 mag) mag u_B-R Uncertainty flag on B-R --- x Relative position to adopted cluster centre (1 pixel = 0.7695 arcsec) pix y Relative position to adopted cluster centre (1 pixel = 0.7695 arcsec) pix mua Proper motion in RA (mu_alpha.cos(delta)) mas/a e_mua Error on mua mas/a mud Proper motion in Dec mas/a e_mud Error on mud mas/a N1 Number of first-epoch plates --- N2 Number of second-epoch plates --- Pr Membership probability % RAh Right Ascension 1950 (hours) (Epoch 1985.5, Perth-70-System, +/- 0.4") h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) (Epoch 1985.5, Perth-70-System, +/- 0.4") --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Francois Ochsenbein CDS 1993 Apr 09 J_A+AS_93_311.xml Four-colour uvby and H-beta photometry of all stars earlier than G0 and brighter than ~10.7mag in Selected Area 203 towards the Chamaeleon-Musca dark clouds J/A+AS/93/373 J/A+AS/93/373 Four-colour uvby and H-beta photometry of all stars Four-colour uvby and H-beta photometry of all stars earlier than G0 and brighter than ~10.7mag in Selected Area 203 towards the Chamaeleon-Musca dark clouds G A P Franco Astron. Astrophys. Suppl. Ser. 93 373 1992 1992A&AS...93..373F ISM: individual (Chamaeleon-Musca clouds) photometry: Stroemgren stars: early-type Results are presented of Stromgren uvby(beta) photometry for 213 stars earlier than G0 and brigher than m sub pg of about 10.7 m in Selected Area 203. The observed area lies close to the geometric center of the Chamaeleon-Musca dark clouds complex. The results yield V, (b-y), m sub 1, c sub 1, and beta on the standard systems, with overall rms errors for one observation of one star of 0.010, 0.004, 0.007, 0.009, and 0.011, respectively.
uvby-beta observations of 213 stars earlier than G0 towards SA 203 SA Designation in Potsdam Spektral-Durchmusterung (Becker & Bruck, Publ. Astrophys, Obs. Potsdam 27-28, 1929-38) --- HD Designation in "Henry Draper" --- MK Spectral classification from Michigan (Houk & Cowley 1975) --- RAh Right Ascension 1900 (hours) h RAm Right Ascension 1900 (minutes) min RAs Right Ascension 1900 (seconds) s DE- Declination 1900 (sign) - DEd Declination 1900 (degrees) deg DEm Declination 1900 (minutes) arcmin V magnitude in Johnson system mag e_V Mean error on V 0.001mag b-y colour index (b-y) mag e_(b-y) Mean error on b-y 0.001mag m1 colour indices difference m1 mag e_m1 Mean error on m1 0.001mag c1 colour indices difference c1 mag e_c1 Mean error on c1 0.001mag o_c Number of nights for uvby observations --- Hbeta Hbeta index mag e_Hbeta Mean error on Hbeta number=1 For star SA 203-377, the "**" in Table 1 has been replaced by the value 99. 0.001mag o_Hbeta Number of nights for Hbeta observations --- UNKNOWN b994 Apr (End) Patricia Bauer [CDS] 26 UNKNOWN UNKNOWN Keypunched at CDS See also Note(1) J_A+AS_93_373.xml UBVRIJHKL photometric catalogue of symbiotic stars J/A+AS/93/383 J/A+AS/93/383 UBVRIJHKL photometric catalogue of symbiotic stars UBVRIJHKL photometric catalogue of symbiotic stars U Munari B F Yudin O G Taranova G Massone F Marang G Roberts H Winkler P A Whitelock Astron. Astrophys. Suppl. Ser. 93 383 1992 1992A&AS...93..383M binaries: symbiotic Photometry stars: colors stars: emission-line, Be stars: variables: general Results are presented of an optical and IR photometric survey of a large sample of symbiotic stars: 93 objects out of the approximately 150 known class members. Attention is given to nearly simultaneous optical and IR observations, and to the observation of a large sample in fixed and well-known photometric systems.
The catalogue (tables 2, 3 and 4) Name Star name --- Type Symbiotic type based on JHK colours: S (star), D (dust), D' (cooler dust) --- Date Observation Date, either as DD-MM-YY or JD --- V Photoelectric observation mag B-V Photoelectric observation mag U-B Photoelectric observation mag V-R Photoelectric observation; R in Johnson or Cousins system mag V-I Photoelectric observation I in Johnson or Cousins system mag System RI filter system: Cousins or Johnson --- K JHKL observation with MkII at SAAO mag u_K Uncertainty flag (:) on K --- J-H JHKL observation with MkII at SAAO mag u_J-H Uncertainty flag (:) on J-H --- H-K JHKL observation with MkII at SAAO mag u_H-K Uncertainty flag (:) on H-K --- K-L JHKL observation with MkII at SAAO mag u_K-L Uncertainty flag (:) on K-L --- James Marcout, Francois Ochsenbein CDS 1994 Feb 22 UNKNOWN UNKNOWN Keypunched at CDS J_A+AS_93_383.xml Optical identifications of faint ultra-steep spectrum radio sources J/A+AS/93/399 J/A+AS/93/399 Optical identifications of faint ultra-steep Optical identifications of faint ultra-steep spectrum radio sources M H Wieringa P Katgert Astron. Astrophys. Suppl. Ser. 93 399 1992 1992A&AS...93..399W galaxies: formation galaxies: radio The first results are reported of an observational study of ultrasteep spectrum (USS) radio sources selected on the basis of Westerbork surveys at 327 MHz complemented by observations at 608 MHz. The study extends the sample of USS sources to sources about 25 times fainter than the 4C sample. The reduction and calibration, optical imaging and spectroscopy, radio sample selection and properties, and optical identifications are discussed. Statistical properties of the sample are investigated, including the magnitude distribution, variations of the identification fraction with spectral index, optical morphology, radio optical position angle differences, and optical spectra. The decrease of the identification fraction with steepening spectral index observed in the 4C sample is present in this sample also. No evidence is found for alignment between the optical and radio axes, and no strong emission lines are found in a subsample for which low-resolution spectroscopy was obtained.
Radio sources with optical CCD data Radio sources without deep CCD images Name The standard name of the object, this corresponds to the name in the middle of the first line above each plot in Fig.3. (note the unconventional naming of the first two sources) --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s e_RA sigma on RA s DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec e_DE sigma on DE arcsec posCode indicates which observation was used for the radio position given: 20A=VLA A-array, 20cm, 20C=VLA C-array 20cm, 49=49cm WSRT, 92=92cm WSRT --- S92 Flux density at 327MHz mJy e_S92 error on S92 mJy S49 Flux density at 608MHz mJy e_S49 error on S49 mJy S20 Flux density at 1490MHz mJy e_S20 error on S20 mJy alpha Weighted spectral index over 327-1490 MHz. --- n_alpha Note on alpha: 'S' for steepening and 'F' for flattening of the spectrum toward higher frequency --- Structure C=Compact/Unresolved sources, E=Extended sources, D=Doubles, T=Triples --- psi Major axis arcsec pa position angle deg R R magnitude (KPNO R-band) of optical candidate mag NoteR Notes for the radio data: + for a steep spectrum source belonging to the sample, - for a source no longer in the sample because or its radio spectrum * indicates a note (see below) --- NoteO Notes for optical data: + for a reliable of highly probable identification - for an empty field (R > 23.5, unless noted otherwise below in the Notes) S identification likely but not certain due to complex radio structure F very faint but probably correct id. P probable id. with radio-optical position difference in the range 2-3" --- Heinz Andernach, Francois Ochsenbein CDS 1993 Jun 11 J_A+AS_93_399.xml An astrometric catalogue of southern and equatorial dwarf novae J/A+AS/93/463 J/A+AS/93/463 An astrometric catalogue of southern and equatoria An astrometric catalogue of southern and equatorial dwarf novae A Bruch J Meijer M Naumann T Schimpke R Ungruhe N Vogt Astron. Astrophys. Suppl. Ser. 93 463 1992 1992A&AS...93..463B binaries: close catalogs novae, cataclysmic variables An astrometric catalog of 116 southern and equatorial dwarf novae is presented. The mean internal accuracy of the coordinates is of the order of +/- 0.025 s in alpha cos delta and +/- 0.3 arcsec in delta. (See J/A+AS/70/481 for the Northern Part) =1987A&AS...70..481B
The catalogue Name variable star name. -- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DEs Declination 1950 (seconds) arcsec DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec e_RA formal (internal) mean error of the measurements at the plate location of the variable star as derived from the least squares solution to the position of the standard stars in right ascension (multiplied by cos(delta)) in seconds of time. number=1 Since Lopez (1985, IBVS 2837) and Williams (1983, ApJS 53, 523) do not quote errors for their measurements no corresponding information can be given for coordinates taken from their publications. s e_DE formal (internal) mean error in declination in seconds of arc. number=1 Since Lopez (1985, IBVS 2837) and Williams (1983, ApJS 53, 523) do not quote errors for their measurements no corresponding information can be given for coordinates taken from their publications. arcsec Epoch epoch of the coordinates. number=2 Since the exact date of the exposures of the SRC plates is not known, we give a mean epoch of 1980 for the corresponding coordinates. Similarly, we do not know the epoch of Lopez's (1985, IBVS 2387)) plates. Therefore, we cannot give values in these cases. yr Source the type of the plate on which the positions were measured, or source of the measurements: L = Lopez (1985, IBVS 2837) W = Williams (1983, ApJS 53, 523) K = Kiplinger (1985, IBVS 2488) Other abbreviations are self-explanatory. --- RefCat Source catalogue for the reference stars. In most cases the AGK3 or the PPM catalogue could be used. However, for some fields we had to use the SAO catalogue which has a somewhat inferior accuracy. --- Nref Number of reference stars for the coordinate determination (only for our own measurements) --- Rem a code for remarks number=3 Code as: 1. The position could not be determined by a Gaussian fit to the stellar image because of close, brighter neighbours. Instead, the position was found by locating the centre of gravitiy of the stellar image visually. 2. There is a difference of more than 5.5 arcsec in right ascension to the position of Lopez (1985, IBVS 2837). 3. On the POSS chart the star is a member of an unresolved group of stars. The position refers to the centre of a Gaussian fitted to this group. 4. Mean values from positions measured on three plates. 5. NN Cen is the northern component of a close optical pair which is not resolved on the chart of Vogt and Bateson (1982, A&AS 48, 383). --- Francois Ochsenbein CDS 1993 Apr 13 J_A+AS_93_463.xml Photoelectric UBV photometry of stars in four fields near the galactic plane. J/A+AS/93/553 J/A+AS/93/553 Photoelectric UBV photometry of stars in four Photoelectric UBV photometry of stars in four fields near the galactic plane. W Saurer K Pfitscher R Weinberger H Hartl Astron. Astrophys. Suppl. Ser. 93 553 1992 1992A&AS...93..553S Galaxy: disk photometry UBV photoelectric data are presented on 170 stars contained in four fields at low Galactic latitude. Finding charts are provided for the four fields.
UBV near Galactic Plane FIELD Field number (I, II, III, IV) --- NUMBER Running number within the field --- RAh Right Ascension (1950) h RAm Right Ascension (1950) min RAs Right Ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec V V magnitude in Johnon's system mag B-V B-V color in Johnon's system mag U-B U-B color in Johnon's system mag CDS 1993 Mar 02 J_A+AS_93_553.xml Multiband analysis of the surface brightness distributions of Sb and Sc spirals CCD images. I. Observations. J/A+AS/93/557 J/A+AS/93/557 Multiband analysis of the surface brightness Multiband analysis of the surface brightness distributions of Sb and Sc spirals CCD images. I. Observations. M Prieto D P T Longley E Perez J E Beckman A M Varela J Cepa Astron. Astrophys. Suppl. Ser. 93 557 1992 1992A&AS...93..557P galaxies: photometry galaxies: spiral galaxies: stellar content Results are presented of an imaging study of eight Sb-Sc spirals, based on CCD observations in the B, V, R, I, and Z photometric filters. Presented are grey scale images, both in individual bands and in color indices, isophote maps, the parameters of the best fits to the isophotes (ellipticity and position angle as functions of deprojected radius), and radial profiles in the passbands. The paper explains how the radial intensity profiles of these galaxies are naturally divisible into inner bulge, outer disk, and an intermediate zone, and it is shown how the color index images can aid in the diagnostics of reddening effects due to older or more metallic stellar population on the one hand, and dust on the other. The data are presented with a view to facilitating the task of dynamically reliable bulge-disk decomposition.
Merged tables 1, 4a and 4b NGC Galaxy designation --- Type Hubble type and luminosity class --- Bt Total apparent blue magnitude corrected for galactic and internal absorption mag M_Bt Total absolute blue magnitude corrected for galactic and internal absorption. mag D Distance, using Ho = 75 km/s/Mpc, from the corrected recession velocity relative to the centroid of the Local Group Mpc R'25 Isophotal major axis distance to 25. mag/arcsec^2 corrected to "face on". arcmin PA(B) Position angle (North eastward) in B filter deg e_PA(B) mean error on PA(B) deg PA(V) Position angle (North eastward) in V filter deg e_PA(V) mean error on PA(V) deg PA(R) Position angle (North eastward) in R filter deg e_PA(R) mean error on PA(R) deg PA(I) Position angle (North eastward) in I filter deg e_PA(I) mean error on PA(I) deg PA(Z) Position angle (North eastward) in Z filter deg e_PA(Z) mean error on PA(Z) deg PA Mean Position angle (North eastward) deg e(B) Disc eccentricity in B filter --- e_e(B) mean error on e(B) --- e(V) Disc eccentricity in V filter --- e_e(V) mean error on e(V) --- e(R) Disc eccentricity in R filter --- e_e(R) mean error on e(R) --- e(I) Disc eccentricity in I filter --- e_e(I) mean error on e(I) --- e(Z) Disc eccentricity in Z filter --- e_e(Z) mean error on e(Z) --- i Mean inclination angle deg Francois Ochsenbein CDS 1993 May 18 J_A+AS_93_557.xml CCD observations in 7 open clusters: NGC 2421,2439,2489,2567,2627,2658,2910 J/A+AS/94/73 J/A+AS/94/73 CCD observations in 7 open clusters: NGC CCD observations in 7 open clusters: NGC 2421,2439,2489,2567,2627,2658,2910 G Ramsay D L Pollaco Astron. Astrophys. Suppl. Ser. 94 73 1992 1992A&AS...94...73R open clusters and associations: general photometry Photometric UBVIc data are presented for the open clusters NGC2439, NGC2489, NGC2567, NGC2627, NGC2658, and NGC2910. From a combination of the new BVIc technique and the analysis of the CMDs, the color excess E(B-V), the distance modulus, and approximate age are given for these clusters and NGC2421. ERRATUM NOTE: in the publication the table headings are in error. The captions of the tables are: Table 7 = NGC 2421 NOT 2439 8 = 2439 2489 9 = 2489 2567 10 = 2567 2627 11 = 2627 2658 12 = 2658 2910 and NGC 2910 was not published as a table, but is present here.
in Table 7 in Table 8 in Table 9 in Table 10 in Table 11 in Table 12 (not present in published paper) Star Running number in cluster --- V Visual magnitude mag B-V Color index mag V-I Color index mag U-B Color index mag Member Membership probability m/pm/pnm/nm/rg --- Av(Q) Reddening derived from the Q technique mag Av(BVI) Reddening derived from the BVIc technique mag Mv Absolute magnitude mag (B-V)0 Intrinsic colors for members and probable members only mag Sp(Q) Spectral type from Q method (only for ngc2421) --- Francois Ochsenbein CDS 1994 Jan 18 Gavin Ramsay J_A+AS_94_73.xml Sample of dumb-bell galaxies in southern rich clusters J/A+AS/95/1 J/A+AS/95/1 Sample of dumb-bell galaxies in southern rich Sample of dumb-bell galaxies in southern rich clusters L Gregorini G Vettolani H R De Ruiter P Parma Astron. Astrophys. Suppl. Ser. 95 1 1992 1992A&AS...95....1G galaxies: clusters: general galaxies: elliptical and lenticular, cD We present two optically selected samples of dumb-bell galaxies extracted from the southern extension of the Abell catalogue and we discuss the selection criteria. The first sample is a volume limited sample obtained by selecting the dumb-bell galaxies in all the 171 clusters within a comoving distance of 210/h Mpc, regardless of Bautz-Morgan classification. The second sample is constituted by dumb-bell systems belonging to the 381 clusters of BM I or I-II type. From the latter sample it is not possible to extract a volume limited sample due to the selection effect present in the Bautz-Morgan classification of the southern Abell catalogue.
dumb-bell systems identified with the brightest cluster member possible dumb-bell systems identified with the brightest cluster member dumb-bell systems identified with cluster members (not the brightest one) ABELL Abell name --- CODIST comoving distance (alternative expression of the unit is "Mpc/(H0/100)" where H0 denotes the Hubble constant) 100km/s q_CODIST the comoving distance is estimated --- RAh right ascension (B1950) of the eastern component of the dumb-bell system (hours) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination of the eastern component of the dumb-bell system (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec D_RAs increment of the second component in RAs s D_DEs increment of the second component in DEs arcsec dumb-bell galaxies belonging to BM I and BM I-II clusters ABELL Abell name --- CODIST comoving distance (alternative expression of the unit is "Mpc/(H0/100)" where H0 denotes the Hubble constant) 100km/s q_CODIST the comoving distance is estimated --- RAh right ascension ((B1950) of the eastern component of the dumb-bell system (hours) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign --- DEd declination of the eastern component of the dumb-bell system (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec D_RAs increment of the second component in RAs s D_DEs increment of the second component in DEs arcsec NOTE 'a'= not the brightest cluster member 'b'= possible dumb-bell 'c'= triple system --- Koichi Nakajima CDS 1993 Nov 20 UNKNOWN UNKNOWN The files were forwarded to CDS by Heinz J. Andernach (courtesy L. Gregorini) J_A+AS_95_1.xml Santiago Fundamental Catalogue. A catalogue of 1105 FK5 stars (equinox J2000.0) J/A+AS/95/355 J/A+AS/95/355 Santiago catalogue of 1105 FK5 stars Santiago Fundamental Catalogue. A catalogue of 1105 FK5 stars (equinox J2000.0) G Carrasco P Loyola Astron. Astrophys. Suppl. Ser. 95 355 1992 1992A&AS...95..355C astrometry declination right ascension stars: FK5 *** No Description Available ***
Santiago Fundamental Catalogue NFK5 Number of the star in the FK5 Catalogue --- n_NFK5 'S' means observation in lower culmination --- DM Durchmusterung number --- Vmag Visual magnitude mag Sp Spectral type --- RAh Right ascension J2000.0 h RAm Right ascension J2000.0 min RAs Right ascension J2000.0 s EPRA Epoch-1900 of right ascension (x 100) yr NRA Number of accepted observations in right ascension --- e_RAs rms uncertainty on right ascension (epsilon_alpha_.cos(delta)) 0.001s pmRA Annual proper motion in right ascension (FK5) s/yr DE- Declination sign --- DEd Declination J2000.0 (when the star was not observed in declination, the FK5 value is given for information). deg DEm Declination J2000.0 arcmin DEs Declination J2000.0 arcsec EPD Epoch-1900 of declination (x 100) yr NDE Number of accepted observations in declination --- ED rms uncertainty on declination 0.01arcsec pmDE Annual proper motion in declination (FK5) arcsec/yr Patricia Bauer CDS 1994 Nov 08 Guillermo Carrasco <gcarrasc@das.uchile.cl> J_A+AS_95_355.xml New grids of stellar models from 0.8 to 120 Msolar at Z=0.020 and Z=0.001 J/A+AS/96/269 J/A+AS/96/269 New grids of stellar models from 0.8 to 120 New grids of stellar models from 0.8 to 120 Msolar at Z=0.020 and Z=0.001 G Schaller D Schaerer G Meynet A Maeder Astron. Astrophys. Suppl. Ser. 96 269 1992 1992A&AS...96..269S stars: evolution stars: mass-loss stars: Wolf-Rayet supergiants *** No Description Available ***
M=120, Z=0.020, with overshooting, standard mass loss M=120, Z=0.020, with overshooting, Mdot x 2 in post-MS M= 85, Z=0.020, with overshooting, standard mass loss M= 85, Z=0.020, with overshooting, Mdot x 2 in post-MS M= 60, Z=0.020, with overshooting, standard mass loss M= 60, Z=0.020, with overshooting, Mdot x 2 in post-MS M= 40, Z=0.020, with overshooting, standard mass loss M= 40, Z=0.020, with overshooting, Mdot x 2 in post-MS M= 25, Z=0.020, with overshooting, standard mass loss M= 25, Z=0.020, with overshooting, Mdot x 2 in post-MS M= 20, Z=0.020, with overshooting, standard mass loss M= 20, Z=0.020, with overshooting, Mdot x 2 in post-MS M= 15, Z=0.020, with overshooting, standard mass loss M= 12, Z=0.020, with overshooting, standard mass loss M= 9, Z=0.020, with overshooting, standard mass loss M= 7, Z=0.020, with overshooting, standard mass loss M= 5, Z=0.020, with overshooting, standard mass loss M= 4, Z=0.020, with overshooting, standard mass loss M= 3, Z=0.020, with overshooting, standard mass loss M=2.5, Z=0.020, with overshooting, standard mass loss M= 2, Z=0.020, with overshooting, standard mass loss M=1.7, Z=0.020, with overshooting, standard mass loss M=1.5, Z=0.020, with overshooting, standard mass loss M=1.25, Z=0.020, with overshooting, standard mass loss M=1.25, Z=0.020, with overshooting, standard mass loss M=1.25, Z=0.020, no overshooting, standard mass loss M= 1, Z=0.020, no overshooting, standard mass loss M=0.9, Z=0.020, no overshooting, standard mass loss M=0.8, Z=0.020, no overshooting, standard mass loss M=120, Z=0.001, with overshooting, standard mass loss M= 85, Z=0.001, with overshooting, standard mass loss M= 60, Z=0.001, with overshooting, standard mass loss M= 40, Z=0.001, with overshooting, standard mass loss M= 25, Z=0.001, with overshooting, standard mass loss M= 20, Z=0.001, with overshooting, standard mass loss M= 15, Z=0.001, with overshooting, standard mass loss M= 12, Z=0.001, with overshooting, standard mass loss M= 9, Z=0.001, with overshooting, standard mass loss M= 7, Z=0.001, with overshooting, standard mass loss M= 5, Z=0.001, with overshooting, standard mass loss M= 4, Z=0.001, with overshooting, standard mass loss M= 3, Z=0.001, with overshooting, standard mass loss M=2.5, Z=0.001, with overshooting, standard mass loss M= 2, Z=0.001, with overshooting, standard mass loss M=1.7, Z=0.001, with overshooting, standard mass loss M=1.5, Z=0.001, with overshooting, standard mass loss M=1.25, Z=0.001,with overshooting standard mass loss M=1.25, Z=0.001, no overshooting, standard mass loss M= 1, Z=0.001, no overshooting, standard mass loss M=0.9, Z=0.001, no overshooting, standard mass loss M=0.8, Z=0.001, no overshooting, standard mass loss NB number of selected point --- Age age yr Mass actual mass in solar masses Sun logL log(luminosity) in solar units Sun logTe log(effective temperature) K X H surface abundance (mass fraction) --- Y He surface abundance (mass fraction) --- C12 12C surface abundance (mass fraction) --- C13 13C surface abundance (mass fraction) --- N14 14N surface abundance (mass fraction) --- O16 16O surface abundance (mass fraction) --- O17 17O surface abundance (mass fraction) --- O18 18O surface abundance (mass fraction) --- Ne20 20Ne surface abundance (mass fraction) --- Ne22 22Ne surface abundance (mass fraction) --- QCC core mass fraction --- logTu log(uncorrected Teff) (WR stars only) K logMdot log(mass loss rate) Sun/yr log(rho_c) log(central density) g/cm3 logTc log(central temperature) K Xc H central abundance (mass fraction) --- Yc He central abundance (mass fraction) --- C12c 12C central abundance (mass fraction) --- C13c 13C central abundance (mass fraction) --- N14c 14N central abundance (mass fraction) --- O16c 16O central abundance (mass fraction) --- O17c 17O central abundance (mass fraction) --- O18c 18O central abundance (mass fraction) --- Ne20c 20Ne central abundance (mass fraction) --- Ne22c 22Ne central abundance (mass fraction) --- Daniel Schaerer Geneva Obs 1993 Sep 07 J_A+AS_96_269.xml Radio spectra of quasars. III. J/A+AS/97/435 J/A+AS/97/435 1410MHz-spectra of quasars III. Radio spectra of quasars. III. Z M Quiniento J C Cersosimo Astron. Astrophys. Suppl. Ser. 97 435-442 1993 1993A&AS...97..435Q VII/54 : Catalogue of extragalactic radio-source identifications (Veron-Cetty & Veron, 1983) VIII/15 : Parkes Radio Sources Catalogue (PKSCAT90) (Wright+ 1990) VIII/16 : The Molonglo Reference Catalogue (MRC) (Large+ 1981) Galaxies, radio Radio sources extragalactic radio sources quasars: general We present the third and final part of the research at 1410MHz for 213 extragalactic objects from the Southern Hemisphere identified as Quasars by Veron-Cetty and Veron (1983A&AS...53..219V). The first (1988A&AS...76...21Q) and second (1990A&AS...83..393Q) parts contained measurement of the flux densities at 1410MHz for 473 sources.
The results of the last part of the Survey Source Name of the source according to IAU --- ModFlag Correction from the publication number=5 this flag is set when corrections have been detected by H. Andernach (see "Modification History" section below) --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec S408 Flux density at 408 MHz number=1 The data are from Molongo Catalogue by Large et al., 1981 =1981MNRAS.194..693L (Catalog <VIII/16>) Jy e_S408 rms uncertainty on S408 Jy Sp1410 Peak flux density at 1410 MHz Jy n_Sp1410 * indicates that no signal was detected --- e_Sp1410 rms uncertainty on Sp1410 Jy alpha1 Spectral index obtained between 408 and 1410 MHz --- S2700 Flux density at 2700 MHz number=2 The data are from Parkes catalogue Jy alpha2 Spectral index obtained between 1410 and 2700 MHz --- S5009 Flux density at 5009 MHz number=2 The data are from Parkes catalogue Jy alpha3 Spectral index obtained between 2700 and 5099 MHz --- C spectral curvature --- z redshift number=3 The redshifts published by Veron-Cetty & Veron (1983; see catalog <VII/54>) where included. These data were modified using 'A catalogue of Quasars and Active Nuclei (2nd Ed.)' (1985), 'A catalogue of Quasars and Active Nuclei (3rd Ed.)', (1980), all of them by Veron-Cetty & Veron --- Vmag visual magnitude Mv obtained and modified with the above publications mag Mabs absolute magnitude number=4 The absolute magnitudes were extracted from Veron-Cetty and Veron (1984, Scientific Rept. No1; 1985 Scientific Rept. No4; 1987, Scientific Rept. No5 and 1989, Scientific Rept. No7) mag Patricia Bauer, Francois Ochsenbein CDS 1996 Apr 18 Thanks are due to Heinz Andernach <hja@hja.vilspa.esa.es> who checked the electronic version, and reported the errors found in the publication flagged UNKNOWN UNKNOWN * The catalogue was keypunched at CDS in 1994, and first documented by Patricia Bauer * 18-Apr-1996: Errors reported by H. Andernach on 28 Feb. 1996 have been applied. Some of these errors, not reported here, concern typo errors of the electronic version compared to the publication. The errors found in the original publication, flagged in the "ModFlag" column, concern the following sources: 1826-782: RA and DE corrected (PKS B1826-782) 1826-782: alpha2 corrected from -0.274 to -2.74 1958-179: Vmag corrected from 26.2 to 18.2 2021-330: DE corrected (PKS B2021-330) 2037-253: alpha1 sign 2058-297: Source name corrected from 2056-297 to 2058-297 2107-105: alpha1 sign 2110-160: RA corrected (PKS B2110-160) 2136-251: DE corrected (MRC B2136-251) 2204-573: alpha1 sign 2221-139: alpha2 sign 2240-107: alpha2 sign 2240-572: alpha1 sign 2345-167: alpha2 sign 2359-14 : alpha1 sign J_A+AS_97_435.xml X-ray emission from thin plasmas. I. Multiple Auger ionisation and fluorescence processes for Be to Zn. J/A+AS/97/443 J/A+AS/97/443 X-ray emission from thin plasmas. I. Multiple X-ray emission from thin plasmas. I. Multiple Auger ionisation and fluorescence processes for Be to Zn. J S Kaastra R Mewe Astron. Astrophys. Suppl. Ser. 97 443 1993 1993A&AS...97..443K atomic data The basic physical processes responsible for X-ray emission from thin plasmas are considered. Collisional ionization or photoionization of inner shells of neutral atoms and ions leads to the creation of a vacancy in one of the inner shells of the ion or atom, which is filled by a cascade of radiative (fluorescent) and nonradiative (Auger) transitions. The net result is the ejection of several electrons and photons, leaving the atom in a multiply ionized state. In this paper, the distribution of the number of emitted photons and electrons after the creation of a hole in an inner shell of an atom or ion is calculated for all ions from H to Zn. The method consists of two stages: the calculation of transition rates for a given electron configuration, and calculation of probabilities of the several cascade sequences using these transition rates.
Electron distribution Z Atomic number --- st Ionisation stage of ion BEFORE ionisation (neutral=1 etc.) --- s Shell number of primary vacancy (1-7 correspond to K L1 L2 L3 M1 M2 M3) --- I Ionisation energy of the primary vacancy in eV (from Lotz) eV E_A Energy that goes into Auger electrons, in eV eV epsilon Correction factor defined in equation 6 of the paper 10-3 PrEj Probability that a photo-ionisation leads to ejection of a total of n electrons, with n running from 1 to 10. NOTE that the probabilities have been multiplied by 10000. 10-4 Fluorescence yields Z Atomic number --- st Ionisation stage of ion BEFORE ionisation (neutral=1 etc.) --- s Shell number of primary vacancy (1-7 correspond to K L1 L2 L3 M1 M2 M3) --- Delta Number of Auger electrons ejected before emission of the line; the line therefore occurs in the ion with ionisation stage st+Delta+1 (the factor 1 corresponds to the photo-electron) --- il Line identification number; labels according to table 1 of the paper. Note that il runs from 1 to 22. --- E Approximate line energy of the transition; note that often more accurate energies can be found in the literature. eV omega The fluorescence yield omega for this line (number of photons emitted per primary vacancy) --- Francois Ochsenbein CDS 1993 Apr 13 J_A+AS_97_443.xml Spectroscopy of 1 Jy and S5 radio source identifications. II. J/A+AS/97/483 J/A+AS/97/483 Spectroscopy of 1 Jy and S5 radio source Spectroscopy of 1 Jy and S5 radio source identifications. II. M Stickel H Kuehr J W Fried Astron. Astrophys. Suppl. Ser. 97 483 1993 1993A&AS...97..483S galaxies: active quasars: emission lines radio continuum: galaxies Low resolution spectroscopy of the optical counterparts is reported for a total of 35 radio sources from the 1 Jy and S5 catalog. We present 24 new redshifts, confirm 2 uncertain redshifts and give spectroscopic data for 6 additional objects with previously known redshifts. While two of the remaining sources turned out to be BL Lac objects showing featureless spectra, the proposed counterpart of one radio source was found to be a galactic star. The correct identification of the latter is a nearby QSO.
Observed 1Jy radio sources Observed S5 radio sources Object Object name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec m Magnitude of the optical identification mag Type Type of the optical identification --- S_5GHz 5GHz flux Jy s(11-6) two-point spectral index between 11 and 6 cm --- fc References to published Finding Charts --- Names Other names --- Journal of 1Jy identifications Line data for 1Jy identifications Object Object name --- Tel Telescope: CA 3.5 = 3.5 m telescope on Calar Alto, Spain LS 2.2 = 2.2 m telescope on La Silla, Chile --- Date Observation date --- iTime Total Integration time s Scale Scale of the wavelength calibrated spectra. 0.1nm/pix Scale2 Scale in in red channel for twin Spectrograph 0.1nm/pix Line data for 1Jy identifications Line data for S5 identifications Object Object name --- z Redshift computed from unweighted z_ind --- Id Element identification --- lam_0 Rest wavwlwngth 0.1nm lam_obs Observed wavwlwngth 0.1nm z_ind Individual redshift --- FWHM FWHM (for emission line) 0.1nm EW Equivalent width (for emission line) 0.1nm Flux Flux (10-16erg/s/cm2) 10-19W/m2 Rem gal = stellar absorption lines of host galaxy --- CDS 1993 Apr 02 J_A+AS_97_483.xml Distribution and studies of the infrared stellar population in the Galaxy. V. Other clear regions around the galactic centre. J/A+AS/97/587 J/A+AS/97/587 JHK photometry of Galactic center stars Distribution and studies of the infrared stellar population in the Galaxy. V. Other clear regions around the galactic centre. R A Ruelas-Mayorga P F Teague Astron. Astrophys. Suppl. Ser. 97 587 1993 1993A&AS...97..587R J/A+AS/93/61 : IR Stellar Population in Baade's window (Ruelas-Mayorga+ 1992) Ruelas-Mayorga, Paper II., 1991RMxAA..22...43R Ruelas-Mayorga & Teague, Paper III., 1992A&AS...93...61R, Cat. <J/A+AS/93/61> Ruelas-Mayorga & Teague, Paper IV., 1992A&AS...95..379R Infrared sources Photometry, infrared Populations, stellar Galaxy: center Galaxy: stellar content We present K-counts and JHK detailed photometry for a number of stars with K<=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga & Teague, 1992A&AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel & Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K<=+9.0, the disk population may be accounted for by those sources with J-K<=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.
Cumulative Counts Functions (CCF) values Region Region number=1 R1: (l,b)=(0.0,-3.5); R2: (l,b)=(0.0,-4.0), R3: (l,b)=(0-0,-4.5) --- Kmagup K magnitude up to which the number of sources has been measured mag Nsources Cumulative number of sources observed --- Corr Corrected number of observed sources --- Ndisk Number of sources per square degree (N) in the disk ct/deg+2 logNdisk LogNdisk [ct/deg+2] logNdisk2 Model-predicted logarithm of Ndisk number=2 Disk parameters: ---------------------------------------------- Region Area R_o_ a(abs) h(abs) a_K_ deg^2^ kpc kpc kpc mag/kpc ---------------------------------------------- R1 0.03857 8.75 4.0 0.1 0.046 R2 0.01563 8.75 4.0 0.1 0.056 R3 0.05143 8.75 4.0 0.1 0.053 ---------------------------------------------- [ct/deg+2] logNbulge logarithm of N for the bulge component [ct/deg+2] logNbulge(BW) logarithm of N derived from the Baade Window bulge CCF and the r^1/4^ law [ct/deg+2] logMean logarithm of the mean of logNbulge and logNbulge(BW) [ct/deg+2] Observed values for the JHK photometry of sources in regions R1, R2 and R3 Region Region designation --- Object Object designation --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Jmag J magnitude mag e_Jmag rms uncertainty on Jmag number=1 When no error is shown, the observational error is 0.02 mag or smaller mag Hmag H magnitude mag e_Hmag rms uncertainty on Hmag number=1 When no error is shown, the observational error is 0.02 mag or smaller mag Kmag K magnitude mag e_Kmag rms uncertainty on Kmag number=1 When no error is shown, the observational error is 0.02 mag or smaller mag J-H J-H colour index mag e_J-H rms uncertainty in J-H mag H-K H-K colour index mag e_H-K rms uncertainty in H-K mag J-K J-K colour index mag e_J-K rms uncertainty in J-K mag James Marcout, Patricia Bauer CDS 1997 Jun 19 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_97_587.xml Carbon Stars in the Small Magellanic Cloud. II. Catalogue of 1707 objects with identifications and spectrophotometry J/A+AS/97/603 J/A+AS/97/603 Carbon Stars in the Small Magellanic Cloud. II. Carbon Stars in the Small Magellanic Cloud. II. Catalogue of 1707 objects with identifications and spectrophotometry E Rebeirot M Azzopardi B E Westerlund Astron. Astrophys. Suppl. Ser. 97 603 1993 1993A&AS...97..603R catalogs Magellanic Clouds stars: carbon surveys Accurate positions and charts for 1707 carbon stars in the Small Magellanic Cloud identified on GRISM plates are presented. The catalog provides data on magnitudes, colors, and carbon-abundance measurements and can be used for selecting carbon stars with special characteristics.
The catalogue of 1707 SMC carbon stars RAW RAW number --- n_RAW An asterisk indicates possible variable star; two asterisks indicate confirmed variable star --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec m1 magnitude measured at 522nm mag u_m1 Uncertainty flag (:) on m1 --- m3-m1 Colour equivalent from measurements at 485nm and 522nm mag u_m3-m1 Uncertainty flag (:) on m3-m1 --- C2(EW) Equivalent width of the C2 band at 516.5nm, measured between the peaks in the spectra at 485 and 522 nm 0.1nm u_C2(EW) Uncertainty flag (:) on C2(EW) --- C2(d) Depth of the C2 band measured from the pseudo-continuum mag u_C2(d) Uncertainty flag (:) on C2(d) --- Rem Remarks number=1 remarks are numbered as follows: 1= Doubtful C star 2= spectrophotometry not possible because of overlapping spectra 3= spectrophotometry not possible because of underexposed spectrum 4= spectrophotometry not possible because of overexposed spectrum 5= very red carbon star 6= very faint carbon star in field A or B and detected at a late stage in the survey by E. Rebeirot 7= medium resolution slit spectroscopy available 8= IR photometry in the Johnson JHK system available --- ABW Cross-identification number=2 acronyms for identifications are ABW = Westerlund et al., 1986 (A&AS 65, 79) BMB = Blanco et al., 1980 (ApJ 242, 938) LEGC = Lloyd Evans et al., 1988 (MNRAS 231, 773) RM = Reid & Mould, 1990 (ApJ 360, 490) NGC 371 = Lloyd Evans, 1978 (MNRAS 183, 305) NGC 419 = Lloyd Evans, 1978 (MNRAS 183, 319), and Azzopardi et al., 1986 (Mess. 43, 12) (AR number) --- Ident Other cross-identifications number=2 acronyms for identifications are ABW = Westerlund et al., 1986 (A&AS 65, 79) BMB = Blanco et al., 1980 (ApJ 242, 938) LEGC = Lloyd Evans et al., 1988 (MNRAS 231, 773) RM = Reid & Mould, 1990 (ApJ 360, 490) NGC 371 = Lloyd Evans, 1978 (MNRAS 183, 305) NGC 419 = Lloyd Evans, 1978 (MNRAS 183, 319), and Azzopardi et al., 1986 (Mess. 43, 12) (AR number) --- Francois Ochsenbein CDS 1993 Jun 11 J_A+AS_97_603.xml Oxygen-rich late-type star lightcurves in the 1-20microm. range. J/A+AS/97/729 J/A+AS/97/729 Oxy-rich late-type star lightcurves in the 1-20 Oxygen-rich late-type star lightcurves in the 1-20microm. range. T Le Bertre Astron. Astrophys. Suppl. Ser. 97 729 1993 1993A&AS...97..729L circumstellar matter stars: AGB and post-AGB stars: late-type stars: mass-loss stars: variables: other supergiants The results of a photometric monitoring in the wavelength range 1-20 mum are presented for 37 oxygen-rich sources. The sample contains optically identified miras (13), M-type supergiants (3), type II OH/IR sources (20) and one unidentified object. Each source was observed on at least 13 occasions (up to 42) over a lapse of at least 1250 days (up to 2150) between 1984 and 1990 with the ESO 1-m telescope equipped with its standard infrared photometer
JHKL'M of 37 sources Name Star designation --- JD Date d J 1.24mum mag H 1.63mum mag K 2.19mum mag L' 3.79mum mag M 4.64mum mag CDS 1993 Mar 30 J_A+AS_97_729.xml A catalogue of K giants at the South Galactic Pole: broadband and DDO photometry and radio velocities J/A+AS/97/835 J/A+AS/97/835 A catalogue of K giants at the South Galactic Pole: A catalogue of K giants at the South Galactic Pole: broadband and DDO photometry and radio velocities C Flynn K C Freeman Astron. Astrophys. Suppl. Ser. 97 835 1993 1993A&AS...97..835F stars: abundances stars: general stars: late-type stars: luminosity function, mass function techniques: radial velocities We describe a sample of K giants at the South Galactic Pole, selected to examine the chemical and kinematical properties of stars perpendicular to the galactic plane and to measure the local column density of the disk. We report velocities, abundances, absolute magnitudes, and broadband BV photometry for over 500 giants.
The results (Table 1 + Table 2) Name The HD or CD number where available; otherwise our own name (no prefix) --- SpT the Michigan Catalog spectral type --- SpL the Michigan Catalog luminosity class --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec C4548 DDO colour index mag C4245 DDO colour index mag C4142 DDO colour index mag o_DDO the number of DDO observations. --- V photoelectric photometry (see column o_BV) mag B-V photoelectric photometry mag o_BV number of BV observations. Stars for which no B-V colour has been quoted have photographic V magnitudes, otherwise everything is photoelectric --- RV heliocentric radial velocity in km/s km/s o_RV number of radial velocity measurements. --- l_[Fe/H] Limit flag (<) on [Fe/H] --- [Fe/H] abundance [Fe/H] from DDO photometry Probable metal weak stars are indicated by [Fe/H] < -1 Sun Mv absolute visual magnitude mag Francois Ochsenbein CDS 1994 Jan 26 Chris Flynn <FLYNN@nbivax.nbi.dk> J_A+AS_97_835.xml uvby-beta photometry of high-velocity and metal-poor stars. VI. A second catalogue, and stellar populations of the Galaxy J/A+AS/97/951 J/A+AS/97/951 uvby-beta photometry of metal-poor stars uvby-beta photometry of high-velocity and metal-poor stars. VI. A second catalogue, and stellar populations of the Galaxy W J Schuster L Parrao M E Contreras Martinez Astron. Astrophys. Suppl. Ser. 97 951 1993 1993A&AS...97..951S Galaxy: evolution Galaxy: kinematics and dynamics photometry: uvby, beta stars: halo stars: high-velocity stars: metal-poor A second catalogue of uvby-beta photometry for 553 high-velocity stars is given; nearly all of these stars come from the Lowell Proper Motion Survey. These data have been taken and reduced using the same photometer, same observing techniques, same standard stars and photometric values, and same reduction programs as the "northern" observations of the first catalogue (Paper I). The errors of these data are very similar to those of the previous catalogue; for most stars the mean errors of V, m1, c1 and beta are less than +/- 0.008 mag., and less than +/- 0.005 mag. for b-y.
The catalogue of uvby-beta photometry Name Designation of the star: G from Giclas, Lowell Proper Motion stars; LTT from Luyten; B from Beers et al., 1985, AJ 90, 2089 --- V on the standard Johnson UBV system mag b-y b-y mag m1 = (v-b) - (b-y) mag c1 = (u-v) - (v-b) mag o_uvby Number of independent observations for indices b-y, m1, c1 --- beta on the standard system mag o_beta Number of independent observations for beta index --- comments indicates a note in the printed document ++ flags too red and/or too evolved four our photometric transformations + flags stars near the limit defined with ++ D indicates that a second fainter star was within or slightly outside the entrance diaphragm CL V magnitudes from Carney & Latham, 1987, AJ 92, 116 taken or averaged with FS V magnitudes from Fouts & Sandage, 19886, AJ 91, 1189 taken or averaged with --- Francois Ochsenbein CDS 1993 Dec 15 The file was kindly provided by William Schuster in December 1993 (schuster@bufadora.astrosen.unam.mx) J_A+AS_97_951.xml The complete sample of 1 Jy BL Lac Objects. II. Observational Data. J/A+AS/98/393 J/A+AS/98/393 1Jy BL Lac Objects: Observational Data The complete sample of 1 Jy BL Lac Objects. II. Observational Data. M Stickel J W Fried H Kuehr Astron. Astrophys. Suppl. 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ASA 5, 1 Wills D., Lynds R., 1978, ApJS 36, 317 Wills D., Wills B.J., 1974, ApJ 190, 271 Wills D., Wills B.J., 1976, ApJS 31, 143 Wills D., Wills B.J., 1979, ApJS 41, 689 Wills D., Wills B.J., Breger M., Hsu J.-C., 1980, AJ 85, 1555 Wright A.E., Ables J.G., Allen D.A., 1983, MNRAS 205, 793 Wyndham J.D., 1966, ApJ 144, 459 Yanni B., York D.G., Gallagher J.S., 1989, ApJ 338, 735 Zekl H., Klare G., Appenzeller I., 1981, A&A 103, 342 BL Lac objects Galaxies, radio Spectroscopy BL Lacertae objects: general radio continuum: galaxies surveys Direct imaging and spectroscopic data are reported for the complete sample of 34 BL Lac objects selected from the 1Jy source catalogue (see Cat. <VIII/5>). A short description of each individual object is given along with a general discussion of the features observed in the optical spectra, the optical morphologies, and the environments of the BL Lac objects.
Basic data for the 1Jy BL Lac objects Object Object name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Vmag Magnitude of the optical identification mag S5GHz 5GHz flux Jy s(11-6) two-point spectral index between 11 and 6 cm --- fc References to published Finding Charts --- r_Object References to BL Lac classification --- l_z Limit flag for redshift --- z redshift --- u_z question mark indicating uncertain redshifts --- r_z References to redshift measurements number=1 Reference are detailed in file refs.dat --- pol maximum optical polarization % r_pol Reference to polarization measurement number=1 Reference are detailed in file refs.dat --- ampl total amplitude of optical variability mag r_ampl Reference to variability measurement number=1 Reference are detailed in file refs.dat --- Names Other names --- References to table1. RefNum =+ Reference number, repeated in more than one line --- Text Text of reference, starting by the 19-digit bibcode --- Journal of the observations Object Object name --- ImDate Observation date of direct image "MM/YY" ImTel Telescope number=1 CA 3.5 = 3.5 m telescope on Calar Alto, Spain CA 2.2 = 2.2 m telescope on Calar Alto, Spain LS 2.2 = 2.2 m telescope on La Silla, Chile --- ImItime Total Integration time s Filter Filter used for direct image --- Seeing Seeing of the direct image arcsec SpDate Observation date of spectrum "MM/YY" SpTel Telescope --- SpItime Total Integration time s Scale Scale of the wavelength calibrated spectra. 0.1nm/pix Scale2 Scale in in red channel for twin Spectrograph 0.1nm/pix Emission and Absorption line data Object Object name --- l_z Limit flag on redshift --- z Redshift computed from unweighted zInd --- Id Element identification --- lam_0 Rest wavelength 0.1nm lam_obs Observed wavelength 0.1nm zInd Individual redshift --- FWHM FWHM (for emission line) 0.1nm EW Equivalent width (for emission line) 0.1nm Flux Flux (10-16erg/s/cm2) 10-19W/m2 Rem gal = stellar absorption lines of host galaxy, abs = intervening absorption line --- Emission line luminosities Object Object name --- z Redshift --- L2798 Mg II 2798 emission line luminosity 10+34W L3727 O II 3727 emission line luminosity 10+34W L5007 O III 5007 emission line luminosity 10+34W l_L6563 Limit flag on LHalpha --- L6563 Halpha/N II emission line luminosity 10+34W Ref Reference for line luminosity number=1 References for this table: 1. Cohen et al. (1977, Mem. R. Astron. Soc. 84, 1) 2. Morris & Ward (1988MNRAS.230..639M) 3. Falomo et al. (1987ApJ...318L..39F) 4. Sitko & Junkkarinen (1985PASP...97.1158S), Lipovetskii et al. (1989, SvA 33, 585) --- Properties of the BL Lac host galaxies Object Object name --- z Redshift --- beta5(B) Profile parameter (blue) --- a/b(B) axial ratio --- PA(B) Position angle of major axis deg re_a(B) effective radius arcsec re(B) effective radius kpc Bmag apparent blue magnitude mag beta5R Profile parameter --- a/b(R) axial ratio --- PA(R) Position angle of major axis deg re_a(R) effective radius arcsec re(R) effective radius kpc Rmag apparent red magnitude mag AV galactic absorption mag Bmag1 apparent blue magnitude (repetition 41-44) mag KB blue K - correction mag MB absolute blue magnitude mag Rmag1 apparent red magnitude (repetition 70-73) mag KR red K - correction mag MR absolute red magnitude mag (B-R) Color Index mag MV absolute visual magnitude (V-R=0.9 assumed) mag MVother other absolute visual magnitude mag Ref Reference to other absolute magnitude number=1 References for this table: 1. Baxter et al. (1987MNRAS.228..313B) 2. Hickson et al. (1982ApJ...258...53H) 3. Ulrich (1989) 4. Smith and Heckman (1989ApJS...69..365S, 1989ApJ...341..658S) 5. Romanishin (1987ApJ...320..586R) 6. Abraham et al. (1991MNRAS.252..482A ) --- Galaxies in the BL Lac fields Object Object name --- limit character for redshift limit from direct image --- l_z lower redshift limit indication --- z Redshift of BL Lac Object --- Nogal galaxy sequence number --- zgal galaxy redshift --- m.gal apparent galaxy magnitude (R - band) mag M.gal absolute galaxy magnitude mag adist apparent distance to the line-of-sight arcsec dist distance to the line-of-sight kpc Rem Remark, see Note number=1 el = redshift derived from emission lines et = early type spectrum (Balmer absorption lines, no 4000A break) abs = redshift derived from absorption lines lt = late type spectrum (4000A break, G - band, MgI - absorption) (a) = redshifts from Cohen et al. (1987ApJ...318..577C) and Yanni et al. (1989ApJ...338..735Y) --- Associations of BL Lac objects with clusters Object Object name --- l_z lower redshift limit indication --- z Redshift of BL Lac Object --- u_z questionable redshift indication --- sep Distance between BL Lac object and cluster arcmin Rcl Distance between BL Lac object and cluster in units of cluster radius --- Cluster cluster designation --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DC Distance class of cluster --- zCl cluster redshift --- Francois Ochsenbein CDS 1993, rev. 28-Aug-1998 Nov 12 J_A+AS_98_393.xml Walraven photometry of stars near the Luminous Blue Variable AG Carinae J/A+AS/98/505 J/A+AS/98/505 Walraven photometry near AG Car Walraven photometry of stars near the Luminous Blue Variable AG Carinae N M Hoekzemal H J G L M Lamers A M van Genderen Astron. Astrophys. Suppl. Ser. 98 505 1993 1993A&AS...98..505H Photometry, VBLUW Stars, early-type dust, extinction photometry stars: colors stars: early-type stars: individual We present Walraven-photometric data of 114 stars of 5.9<V<14.7 within 17 arcmin of the Luminous Blue Variable AG Car (HD 94910). The results are expressed in terms of V-magnitude in the Johnson system and in observed and extinction-free colours in the Walraven system. For a description of the Walraven photometric system, see e.g. <GCPD/11>
AG Car HD 94910 10 56 11.6 -60 27 13
Program stars RAh Right ascension number=1 The coordinates are derived from the telescope setting; the 1988 equinox is assumed, the DE seems to be in error by 11' (11' should be substracted to get 1988 Declination). The accuracy is +/-4s in RA, +/-.005deg in DE h RAm Right ascension number=1 The coordinates are derived from the telescope setting; the 1988 equinox is assumed, the DE seems to be in error by 11' (11' should be substracted to get 1988 Declination). The accuracy is +/-4s in RA, +/-.005deg in DE min RAs Right ascension number=1 The coordinates are derived from the telescope setting; the 1988 equinox is assumed, the DE seems to be in error by 11' (11' should be substracted to get 1988 Declination). The accuracy is +/-4s in RA, +/-.005deg in DE s DE- Declination sign --- DEdeg Declination number=1 The coordinates are derived from the telescope setting; the 1988 equinox is assumed, the DE seems to be in error by 11' (11' should be substracted to get 1988 Declination). The accuracy is +/-4s in RA, +/-.005deg in DE deg Name Star name --- Vmag Johnson-V magnitude mag Walraven photometry Name Star name --- HJD Heliocentric Julian date d Vmag Walraven V magnitude mag (V-B) Observed (V-B) colour index in Walraven system mag (B-U) Observed (B-U) colour index in Walraven system mag (U-W) Observed (U-W) colour index in Walraven system mag (B-L) Observed (B-L) colour index in Walraven system mag q_Vmag Quality factor on V Walraven-filter number=1 The quality range from 0=excellent to 9=unreliable. * indicates a faulty measurement --- q_Bmag Quality factor on B Walraven-filter number=1 The quality range from 0=excellent to 9=unreliable. * indicates a faulty measurement --- q_Lmag Quality factor on L Walraven-filter number=1 The quality range from 0=excellent to 9=unreliable. * indicates a faulty measurement --- q_Umag Quality factor on U Walraven-filter number=1 The quality range from 0=excellent to 9=unreliable. * indicates a faulty measurement --- q_Wmag Quality factor on W Walraven-filter number=1 The quality range from 0=excellent to 9=unreliable. * indicates a faulty measurement --- Obs Observers number=2 NMH: Hoekzema, LAR: Larsen, WAN: Wanders --- [B-U] Extintion-free colour [B-U] mag [U-W] Extintion-free colour [U-W] mag [B-L] Extintion-free colour [B-L] mag {B-L} Extintion-free colour {B-L} mag James Marcout, Patricia Bauer CDS 1997 Feb 19 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_A+AS_98_505.xml Grids of stellar models. II. From 0.8 to 120 Msolar at Z=0.008 J/A+AS/98/523 J/A+AS/98/523 Grids of stellar models. II. From 0.8 to 120 Grids of stellar models. II. From 0.8 to 120 Msolar at Z=0.008 D Schaerer G Meynet A Maeder G Schaller Astron. Astrophys. Suppl. Ser. 98 523 1993 1993A&AS...98..523S Hertzsprung-Russell (HR diagram) Magellanic Clouds stars: evolution *** No Description Available ***
M=120, z = 0.008, with overshooting, standard mass loss M=85, z = 0.008, with overshooting, standard mass loss M=60, z = 0.008, with overshooting, standard mass loss M=40, z = 0.008, with overshooting, standard mass loss M=25, z = 0.008, with overshooting, standard mass loss M=20, z = 0.008, with overshooting, standard mass loss M=15, z = 0.008, with overshooting, standard mass loss M=12, z = 0.008, with overshooting, standard mass loss M=10, z = 0.008, with overshooting, standard mass loss M=7, z = 0.008, with overshooting, standard mass loss M=5, z = 0.008, with overshooting, standard mass loss M=4, z = 0.008, with overshooting, standard mass loss M=3, z = 0.008, with overshooting, standard mass loss M=2.5, z = 0.008, with overshooting, standard mass loss M=2, z = 0.008, with overshooting, standard mass loss M=1.7, z = 0.008, with overshooting, standard mass loss M=1.5, z = 0.008, with overshooting, standard mass loss M=1.25, z = 0.008, with overshooting standard mass loss M=1.25, z = 0.008, no overshooting standard mass loss M=1, z = 0.008, no overshooting, standard mass loss M=0.9, z = 0.008, no overshooting, standard mass loss M=0.8, z = 0.008, no overshooting, standard mass loss NB number of selected point --- Age age yr Mass actual mass in solar masses Sun logL log(luminosity) in solar units Sun logTe log(effective temperature) K X H surface abundance (mass fraction) --- Y He surface abundance (mass fraction) --- C12 12C surface abundance (mass fraction) --- C13 13C surface abundance (mass fraction) --- N14 14N surface abundance (mass fraction) --- O16 16O surface abundance (mass fraction) --- O17 17O surface abundance (mass fraction) --- O18 18O surface abundance (mass fraction) --- Ne20 20Ne surface abundance (mass fraction) --- Ne22 22Ne surface abundance (mass fraction) --- QCC core mass fraction --- logTu log(uncorrected Teff) (WR stars only) K logMdot log(mass loss rate) Sun/yr log(rho_c) log(central density) g/cm3 logTc log(central temperature) K Xc H central abundance (mass fraction) --- Yc He central abundance (mass fraction) --- C12c 12C central abundance (mass fraction) --- C13c 13C central abundance (mass fraction) --- N14c 14N central abundance (mass fraction) --- O16c 16O central abundance (mass fraction) --- O17c 17O central abundance (mass fraction) --- O18c 18O central abundance (mass fraction) --- Ne20c 20Ne central abundance (mass fraction) --- Ne22c 22Ne central abundance (mass fraction) --- Daniel Schaerer Geneva Obs 1993 Sep 07 J_A+AS_98_523.xml IRAS Sources behind the Solar circle. III. Observations of H2O, OH, CH3OH and CO J/A+AS/98/589 J/A+AS/98/589 IRAS Sources behind the Solar circle. III. Obs IRAS Sources behind the Solar circle. III. Observations of H2O, OH, CH3OH and CO J G A Wouterloot J Brand K Fiegle Astron. Astrophys. Suppl. Ser. 98 589 1993 1993A&AS...98..589W ISM: molecules masers radio lines: molecular We have used the 100-m Effelsberg and 32-m Medicina radiotelescopes to search for H2O maser emission (22.235 GHz) towards 1143 IRAS sources, for OH (1665/67 MHz) towards 303 IRAS sources, and for CH3OH (12.179 GHz) towards 19 IRAS sources. The IRAS sources have been selected to have colors of premain sequence objects. To obtain an estimate of the kinematic distance, we observed (C-12)O (J = 2 to 1) and (C-12)O (J = 3 to 2) with the KOSMA 3-m telescope towards 25 sources showing H2O emission and not yet observed in CO. This paper presents the observational results in form of tables with line parameters or upper limits and spectra of detected sources.
IRAS
Line parameters towards IRAS sources observed in H2O IRAS IRAS denomination --- Name other name --- sigmaH2O rms per channel of the spectrum taken on a given day (H2O result) Jy n_sigmaH2O resolution of the spectra a: 0.64 km/s b: 0.32 km/s c: 0.16 km/s d: 0.08 km/s e: 0.04 km/s f: 0.02 km/s --- V(H2O) LSR velocity of the strongest maser feature (H2O result) km/s n_V(H2O) a '*' indicates value unknown ---- F*L(H2O) peak flux density of the strongest feature (H2O result) Jy Vmin(H2O) velocity range V_low, where emission is detected (H2O result) km/s n_Vmin(H2O) a '*' indicates value unknown ---- Vmax(H2O) velocity range V_high where emission is detected (H2O result) km/s n_Vmax(H2O) a '*' indicates value unknown --- I(F*L(H2O)) integrated flux density (H2O result) Jy.km/s L(H2O) H2O luminosity Sun Obs date of observation "DD/MM/YY" r_Obs references for observation: (1): this paper; (2): WW; (3): WBH; (4):KJB; (5): CWC; (6): PBC --- n_CO rms value if no CO has been detected --- V(CO) radial velocity (CO result) km/s d(CO) kinematic distance (CO result) kpc LFIR total FIR luminosity Sun Positions of H2O masers IRAS IRAS denomination --- n_IRAS a 'n' denotes no IRAS --- RAh1 right ascension 1950 for IRAS position h RAm1 right ascension 1950 for IRAS position min RAs1 right ascension 1950 for IRAS position s DEd1 declination 1950 for IRAS position deg DEm1 declination 1950 for IRAS position arcmin DEs1 declination 1950 for IRAS position arcsec RAh2 right ascension 1950 for H2O maser position h RAm2 right ascension 1950 for H2O maser position min RAs2 right ascension 1950 for H2O maser position s DEd2 declination 1950 for H2O maser position deg DEm2 declination 1950 for H2O maser position arcmin DEs2 declination 1950 for H2O maser position arcsec Rem. remarks --- Sources observed in OH IRAS IRAS denomination number= IRAS05358+3543 spectrum published by WBH IRAS18174-1612, BE45, M17(4) maser emission possibly from BE48, 0.5' away BE46, M17(1) maser emission possibly from BE48, 3.2' away IRAS18174-1612, BE47, M17(2) maser emission possibly from BE48, 0.3' away BE52 maser emission possibly from BE51, 1.4' away IRAS18244-1155, BE56 maser emission possibly from BE57, 6.0' away IRAS18449-0115, BE79 known maser; see BE BE81, W43(M2) maser emission possibly from BE84, 4.4' away IRAS19209+1421, BE114, W51W maser emission possibly from W51M, 8.9' away IRAS21306+5540 spectrum published by WBH IRAS22566+5830, S152 spectrum published by WW --- Name other name number= IRAS05358+3543 spectrum published by WBH IRAS18174-1612, BE45, M17(4) maser emission possibly from BE48, 0.5' away BE46, M17(1) maser emission possibly from BE48, 3.2' away IRAS18174-1612, BE47, M17(2) maser emission possibly from BE48, 0.3' away BE52 maser emission possibly from BE51, 1.4' away IRAS18244-1155, BE56 maser emission possibly from BE57, 6.0' away IRAS18449-0115, BE79 known maser; see BE BE81, W43(M2) maser emission possibly from BE84, 4.4' away IRAS19209+1421, BE114, W51W maser emission possibly from W51M, 8.9' away IRAS21306+5540 spectrum published by WBH IRAS22566+5830, S152 spectrum published by WW --- H2O H2O detected (+) or not detected (-) number= IRAS05358+3543 spectrum published by WBH IRAS18174-1612, BE45, M17(4) maser emission possibly from BE48, 0.5' away BE46, M17(1) maser emission possibly from BE48, 3.2' away IRAS18174-1612, BE47, M17(2) maser emission possibly from BE48, 0.3' away BE52 maser emission possibly from BE51, 1.4' away IRAS18244-1155, BE56 maser emission possibly from BE57, 6.0' away IRAS18449-0115, BE79 known maser; see BE BE81, W43(M2) maser emission possibly from BE84, 4.4' away IRAS19209+1421, BE114, W51W maser emission possibly from W51M, 8.9' away IRAS21306+5540 spectrum published by WBH IRAS22566+5830, S152 spectrum published by WW --- r_H2O reference for H2O detection, (1): this paper, (2): WW, (3): WBH, (4): Be number= IRAS05358+3543 spectrum published by WBH IRAS18174-1612, BE45, M17(4) maser emission possibly from BE48, 0.5' away BE46, M17(1) maser emission possibly from BE48, 3.2' away IRAS18174-1612, BE47, M17(2) maser emission possibly from BE48, 0.3' away BE52 maser emission possibly from BE51, 1.4' away IRAS18244-1155, BE56 maser emission possibly from BE57, 6.0' away IRAS18449-0115, BE79 known maser; see BE BE81, W43(M2) maser emission possibly from BE84, 4.4' away IRAS19209+1421, BE114, W51W maser emission possibly from W51M, 8.9' away IRAS21306+5540 spectrum published by WBH IRAS22566+5830, S152 spectrum published by WW --- 1665 OH result for 1665 MHz M: maser emission, A: absorption, -: not detected number= IRAS05358+3543 spectrum published by WBH IRAS18174-1612, BE45, M17(4) maser emission possibly from BE48, 0.5' away BE46, M17(1) maser emission possibly from BE48, 3.2' away IRAS18174-1612, BE47, M17(2) maser emission possibly from BE48, 0.3' away BE52 maser emission possibly from BE51, 1.4' away IRAS18244-1155, BE56 maser emission possibly from BE57, 6.0' away IRAS18449-0115, BE79 known maser; see BE BE81, W43(M2) maser emission possibly from BE84, 4.4' away IRAS19209+1421, BE114, W51W maser emission possibly from W51M, 8.9' away IRAS21306+5540 spectrum published by WBH IRAS22566+5830, S152 spectrum published by WW --- 1667 OH result for 1667 MHz M: maser emission, A: absorption, E: thermal emission, -: not detected blank: not observed number= IRAS05358+3543 spectrum published by WBH IRAS18174-1612, BE45, M17(4) maser emission possibly from BE48, 0.5' away BE46, M17(1) maser emission possibly from BE48, 3.2' away IRAS18174-1612, BE47, M17(2) maser emission possibly from BE48, 0.3' away BE52 maser emission possibly from BE51, 1.4' away IRAS18244-1155, BE56 maser emission possibly from BE57, 6.0' away IRAS18449-0115, BE79 known maser; see BE BE81, W43(M2) maser emission possibly from BE84, 4.4' away IRAS19209+1421, BE114, W51W maser emission possibly from W51M, 8.9' away IRAS21306+5540 spectrum published by WBH IRAS22566+5830, S152 spectrum published by WW --- Parameters of OH maser emission IRAS IRAS name --- Freq. frequency MHz FL1 LCP peak flux density Jy VLSR1 LCP LSR velocity of the strongest maser feature km/s Vmin1 LCP velocity range V_low where emission is detected km/s Vmax1 LCP velocity range V_high where emission is detected km/s I(FL1) LCP integrated flux density Jy.km/s FL2 RCP peak flux density Jy VLSR2 RCP LSR velocity of the strongest maser feature km/s Vmin2 RCP velocity range V_low where emission is detected km/s Vmax2 RCP velocity range V_high where emission is detected km/s Fint2 RCP integrated flux density Jy.km/s Positions of OH masers IRAS IRAS name --- RAh right ascension 1950 for OH maser position h RAm right ascension 1950 for OH maser position min RAs right ascension 1950 for OH maser position s DE- declination sign --- DEd declination 1950 for OH maser position deg DEm declination 1950 for OH maser position arcmin DEs declination 1950 for OH maser position arcsec Rem. remarks --- Parameters of OH thermal absorption or emission Name IRAS or BE denomination --- Freq. frequency MHz Tmb brightness temperature K VLSR LSR velocity km/s e_VLSR uncertainty of LSR velocity km/s DeltaV linewidth km/s e_DeltaV uncertainty of linewidth km/s I(Tmb) brightness temperature integrated over velocity K.mk/s e_I(Tmb) rms uncertainty on I(Tmb) K.mk/s Rem. remarks --- CH3OH observations IRAS IRAS denomination --- GLON galactic longitude deg GLAT galactic latitude deg sigma rms Jy DeltaV resolution of spectra km/s Date observation date "DD/MM/YY" 12CO(2-1) observations IRAS IRAS denomination --- TR* temperature K n_TR* a '*' denotes that rms = 0.2 when TR* is not detected --- e_TR* rms uncertainty on TR* K VLSR LSR velocity km/s e_VLSR uncertainty of LSR velocity km/s DeltaV linewidth km/s e_DeltaV uncertainty of linewidth km/s Rem. remarks number=1 as dist: for these sources we assumed a distance of 0.35 kpc nk dist: for these sources we used the near kinematic distances --- R distance from galactic centre kpc d distance from Sun kpc z distance from galactic plane pc LFIR FIR luminosity Sun Name other name --- Francois Ochsenbein CDS 1994 Jan 12 Jan Wouterloot J_A+AS_98_589.xml The Miyun 232 MHz survey. I. Fields centred at RA: 00h41m, Dec: 41{deg}12' and RA: 07h00m, Dec: 35{deg}00' J/A+AS/99/545 J/A+AS/99/545 The Miyun 232 MHz survey. I The Miyun 232 MHz survey. I. Fields centred at RA: 00h41m, Dec: 41{deg}12' and RA: 07h00m, Dec: 35{deg}00' X Zhang Y Zhen H Chen S Wang Astron. Astrophys. Suppl. Ser. 99 545 1993 1993A&AS...99..545Z J/A+AS/121/59 : Miyun 232MHz survey (Zhang+ 1997) J/other/AcApS/16.103 : Miyun 232 MHz survey. II. The main list (Zhang+ 1996) Radio continuum Radio sources Surveys radio sources: general surveys This catalogue contains a new meter-wave survey of the sky region north of declination 30{deg}, carried out with the Miyun 232 MHz SSSynthesis Radio Telescope (MSRT) at HPBW 3.8' x 3.8' cosec(dec). Results from two fields are presented here; the fields are 8 degrees on a side, centered at 0041+41.2 and 0700+35.0. The accuracy of flux determination is limited by background fluctuation which is about 30 mJy. The catalogue is complete for sources with flux greater than 0.25 Jy. The total number of sources listed in the catalogue is 687.
Miyun 232 MHz Survey of Two Fields: 0041+41.2 and 0700+35.0 Name Name of source number=1 This column gives the name of the source, comprised of the letters "MY" followed by the hours and minutes of right ascension, the sign of the declination, and the degrees, to the nearest tenth of a degree. --- RAh Right Ascension (B1950) (hour) number=2 These columns give the B1950 position of the source, Errors in position were estimated in three ways and the resulting rms of position errors can be expressed as RA_err (arcsec) = 5" / S (Jy) Dec_err = RA_err * cosec(Dec) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=2 These columns give the B1950 position of the source, Errors in position were estimated in three ways and the resulting rms of position errors can be expressed as RA_err (arcsec) = 5" / S (Jy) Dec_err = RA_err * cosec(Dec) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec S232p Peak flux density in Jy number=3 These columns give the peak flux density and the integrated flux density of the source, in Jy. The flux density scale of Baars et al. (1977A&A....61...99B) has been used. Errors in flux density were also estimated by three different methods: (a) the Monte-Carlo method, which serves to estimate the degradation of position and flux accuracy by background noise; (b) method of direct comparison, ie, comparing the observed data with well-chosen references; and (c) experimental formulas. Monte Carlo experiments were used at four different levels, i.e. 0.7 Jy, 1.0 Jy, 1.5 Jy and 2.0 Jy. From the results, the uncertainty of flux density was found to be independent of the artificial sources. These results showed that about 60% of the sources had apparent flux densities within +/-30 mJy of their "true" flux densities. Jy S232i Integrated flux density number=3 These columns give the peak flux density and the integrated flux density of the source, in Jy. The flux density scale of Baars et al. (1977A&A....61...99B) has been used. Errors in flux density were also estimated by three different methods: (a) the Monte-Carlo method, which serves to estimate the degradation of position and flux accuracy by background noise; (b) method of direct comparison, ie, comparing the observed data with well-chosen references; and (c) experimental formulas. Monte Carlo experiments were used at four different levels, i.e. 0.7 Jy, 1.0 Jy, 1.5 Jy and 2.0 Jy. From the results, the uncertainty of flux density was found to be independent of the artificial sources. These results showed that about 60% of the sources had apparent flux densities within +/-30 mJy of their "true" flux densities. Jy Bkgr Local background level around source number=4 This column gives the local zero level (in Jy), i.e. the average background level near the source. Jy GB87name Name from 1987 Green Bank Catalogue number=5 This column gives the source name from the 1987 Green Bank Catalogue (Gregory and Condon 1991ApJS...75.1011G) (Cat. <VIII/14>) in the same IAU-format as in column 1 of the present data table [note that the original 87GB does NOT present IAU-names and that truncation to a tenth of a degree might lead to non-unique names!]. --- Sp+Index Estimated spectral index from 232-4850 MHz number=6 This column gives the estimated spectral index between 232 MHz and 4850 MHz. Alpha is defined in the sense S {prop.to} {nu}^{alpha}^. --- Patricio Ortiz CDS 1999 Mar 30 UNKNOWN UNKNOWN Prepared from the tables available at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) J_A+AS_99_545.xml UBV photometry of galactic foreground and LMC member stars. I. Galactic foreground stars J/A+AS/99/591 J/A+AS/99/591 UBV photometry of LMC foreground stars UBV photometry of galactic foreground and LMC member stars. I. Galactic foreground stars J Gochermann H -G Grothues M O Oestreicher T W Berghoefer T Schmidt-Kaler Astron. Astrophys. Suppl. Ser. 99 591 1993 1993A&AS...99..591G J/A+AS/121/243 : GPM1 catalogue (Rybka+ 1997) Ardeberg A., Brunet J.P., Maurice E., Prevot L. 1972, A&AS 6, 249 =1972A&AS....6..249A Feast M.W., Thackeray A.D., Wesselink A.J. 1960, MNRAS 124, 337 =1960MNRAS.121..337F Fehrenbach Ch., Duflot M. 1970, A&A Spec. Suppl. 1, 1 (and continuations) =1970A&ASS...1....1F =1973A&AS...10..231F =1981A&AS...46...13F Leavitt H.S. 1908, Harvard Ann. 60, 87 Nicolet B. 1978, A&AS 34, 1 =1978A&AS...34....1N Magellanic Clouds Photometry, UBV Galaxy: stellar content Magellanic Clouds photometry: UBV UBV photometry of 955 galactic foreground stars in the direction to the Large Magellanic Cloud is presented. The stars have been chosen from foreground star catalogues and have been measured to complete a new data base containing entries of more than 5000 stars in the direction of the LMC. First and second order extinction coefficients at La Silla/Chile are given, which differ from the standard values because of the 1991 eruption of the volcano Mt. Pinatubo.
Johnson UBV photometries of LMC galactic foreground stars PV Number from Fehrenbach & Duflot (1970) --- HD HD/HDE number --- Name Other identifiers given in catalogues of foreground and member stars, as well as in the Harvard Variable list number=1 the acronyms are: A = Ardeberg (1972) S = Fehrenbach & Duflot (1970) supplement, uncertain membership RV = Feast et al. (1960) HV = Harvard Variable No., Leavitt (1908) --- o_Vmag Number of measurements --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V color index mag e_B-V rms uncertainty on B-V mag U-B U-B color index mag e_U-B rms uncertainty on B-V mag q_Vmag Quality of V as defined by Nicolet (1978) --- q_B-V Quality of B-V as defined by Nicolet (1978) --- q_U-B Quality of U-B as defined by Nicolet (1978) --- Rem An asterisk indicates a remark number=2 Stars referenced by their P number in Fehrenbach & Duflot (1970): 385 Variable HV 5509 450 Wrong Hodge & Wright number given by Fehrenbach & Duflot (1970): not 29/94 but 29/95 486 Double star (dist. approx. 4''; both components only measured in common 663 Variable HV 5650 827 Variable HV 2435 1013 Double star (dist. approx. 2"); both components only measured in common; HDE 269526 is listed as FD 1013 and FD 1014 by Fehrenbach & Duflot (1970): components of binary (?) 1045 U-B has been measured only twice 1054 Close binary (Feast et al. 1960: dist. = 1"), both components only measured in common 1190 Star lies at the edge of a nebula 1253 Identification as HDE 269939 by Fehrenbach & Duflot (1970) is correct; HDE is numbered twice (cf. FD 1259) 1259 Identification as HDE 269939 by Fehrenbach & Duflot (1970) is not correct 1356 Variable HV 6024 1641 Wrong Hodge & Wright number given by Fehrenbach & Duflot (1970): not 61/64 but 61/60 1646 Wrong Hodge & Wright number given by Fehrenbach & Duflot (1970): not 61/60 but 61/64 2003 Double star ? HD36705 Short period variable with a period of approx. 12 hours, amplitude in V = 0.09 mag; measurements were obtained on November 29, 1991 --- Patricia Bauer CDS 1996 May 28 We thank Hans-Georg Grothues <hgg@astro.ruhr-uni-bochum.de> for having provided the data in electronic form. J_A+AS_99_591.xml CCD Surface Photometry of galaxies with dynamical data II. UBR photometry of 39 elliptical galaxies J/AJ/100/1091 J/AJ/100/1091 UBR photometry of 39 elliptical galaxies CCD Surface Photometry of galaxies with dynamical data II. UBR photometry of 39 elliptical galaxies R F Peletier R L Davies G D Illingworth L E Davis M Cawson Astron. J. 100 1091 1990 1990AJ....100.1091P Galaxies, optical Photometry, CCD We have obtained U,B, and R CCD surface photometry for a sample of 39 elliptical galaxies. For each galaxy we have determined the surface brightness profile, U-R and B-R color profiles, and the ellipticity and position angle profiles, all as function of major axis radius, using a two-dimensional ellipse fitting program. In addition, we have derived the sin and cos(3.theta) and 4.theta terms that describe the high-order deviations of the B and R isophotes from ellipses. While it is very common for ellipticals to display measurable 3.theta and 4.theta terms, the amplitudes of these terms rarely exceed 0.5%. The isophotes of elliptical galaxies are very well characterized by ellipses. The surface brightness and color profiles are given to radii at which the error in the profile reaches 0.1 mag from the uncertainty in the brightness of the night sky. We have carried out a series of simulations of the effects of seeing on luminosity and ellipticity profiles, to determine the radius beyond which the errors in our data from seeing are less than 0.05 mag and 0.02 in ellipticity. Measurable effects of seeing extend to surprisingly large radii, as much as 5-10 seeing radii, depending upon the ellipticity of the galaxy and the form of the surface brightness profile. Ellipticity and position angle profiles are usually the same in all passbands with no indication that the contours of constant color are more or less flattened than the isophotes, i.e., the isochromes and isophotes have the same shapes, but the insensitivity of the ellipticity to differences between these properties makes this a weak argument. The high-order terms, particularly the 3.theta terms, appear to be sensitive diagnostics for the existence of dust in ellipticals. We find that all the galaxies in this sample either become bluer in B-R and U-R with increasing radius or are of constant color. Mean values for the logarithmic gradients in color are -0.09 mag/arcsec2 per dex in radius in B-R, and -0.20 mag/arcsec2 per dex in radius in U-R. These color changes are consistent with a decrease in the [Fe/H] of approximately 0.20 per decade in radius. Surprisingly, there is no correlation of color gradient with luminosity. It is striking, however, that the lowest luminosity galaxies in the sample (i.e., those with M(B) > -20) do not show any color gradients. They have boxy isophotes, and are also rotationally flattened. While these properties may be related to the fact that they are companions of larger ellipsoidal systems, it could provide an important clue to the formation of ellipticals. Low luminosity ellipticals that are not close companions to giant ellipticals need to be studied. List of the 39 galaxies observed: NGC 315 NGC 720 NGC 741 NGC 1052 NGC 1129 NGC 1600 Abell 496 NGC 2300 NGC 2768 NGC 2778 NGC 2832 NGC 3377 NGC 3379 NGC 3605 NGC 3665 NGC 3801 NGC 4261 NGC 4278 NGC 4374 NGC 4387 NGC 4406 NGC 4472 NGC 4478 NGC 4486 NGC 4551 NGC 4636 NGC 4649 NGC 4697 NGC 4874 NGC 4889 NGC 5638 NGC 5813 NGC 5831 NGC 5845 IC 1101 NGC 6051 NGC 6086 NGC 6269 NGC 7626
Galaxy Parameters Name Name of the elliptical galaxies --- n_mag magnitude band --- Radius Radius along the major axis arcsec mag R, B or U magnitude depending on m_mag mag/arcsec2 Ell Ellipticity = 1-b/a --- PosAngl Position Angle from N to E deg Sin3 3{theta} term in Fourier expansion of isophote shape mag/arcsec2 Cos3 3{theta} term in Fourier expansion of isophote shape mag/arcsec2 Sin4 4{theta} term in Fourier expansion of isophote shape mag/arcsec2 Cos4 4{theta} term in Fourier expansion of isophote shape mag/arcsec2 B-R B-R color mag/arcsec2 U-R U-R color mag/arcsec2 Joseph Florsch CDS 1994 Apr 06 Reynier Peletier <peletier@cfa.harvard.edu> J_AJ_100_1091.xml Ruprecht 106: a young metal-poor galactic globular cluster. J/AJ/100/1811 J/AJ/100/1811 Ruprecht 106: a young metal-poor galactic Ruprecht 106: a young metal-poor galactic globular cluster. R Buonanno G Buscema F Fusi Pecci H B Richer G G Fahlman Astron. J. 100 1811 1990 1990AJ....100.1811B Clusters, globular Photometry, BV UBV CCD photometry for about 2500 stars in the Galactic globular cluster Ruprecht 106 has been performed yielding the first color-magnitude diagram (CMD) for this object. The CMD extends down to about 2 mag fainter than the main-sequence turnoff (TO). The cluster possesses a remarkably flat horizontal branch which lies completely to the red of the instability strip. From the analysis of the CMD the following basic parameters have been determined: [Fe/H] = -1.09 and primordial helium abundance Yp = 0.20 0.05. A sizable, highly centrally concentrated population of blue stragglers has also been detected. The location and morphology of the mean ridge lines in the CMD of Ruprecht 106 have then been differentially compared with that of the metal-rich cluster 47 Tuc, NGC 362, a cluster of intermediate metallicity, and with two well-studied metal-poor clusters, M68 and NGC 6397. Significant differences in the positions of the TOs are apparent in the comparison with the metal-poor clusters. These differences can be explained if Ruprecht 106 is 4-5 Gyr younger than NGC 6397 and M68, although alternative, less straightforward explanations cannot be ruled out. The horizontal branch morphology fits perfectly into this picture using models with non-solar-scaled abundances ([O/Fe]>0.5), showing that two second parameters are at work in this cluster, i.e., age (the dominant) and O enhancement. If these findings are confirmed, Ruprecht 106 will turn out to be the first young metal-poor Galactic globular cluster discovered, with quite strong implications for the study of the collapse and enrichment of the Galactic halo. Notes: Field1 is centered on the cluster center (12 35 53 -50 52.6 1950). Field2 is located 2.7arcmin east of Field1,
Field1 (cluster center) N1 Number in Field1 (in Simbad: Cl* Ruprecht 106 BBF 1-N1) --- V magnitude mag B-V color index mag X position toward N arcsec Y position toward W arcsec Field2 (2.7arcmin east) N2 Number in Field2 (in Simbad: Cl* Ruprecht 106 BBF 2-N2) --- V magnitude mag B-V color index mag X position toward N arcsec Y position toward W arcsec M.J. Wagner Francois Ochsenbein CDS 1994 Apr 15 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_100_1811.xml Massive stars in Cyg OB2. J/AJ/101/1408 J/AJ/101/1408 Massive stars in Cyg OB2. Massive stars in Cyg OB2. P Massey A B Thompson Astron. J. 101 1408 1991 1991AJ....101.1408M J/A+AS/111/407 : VI Cygni red + reddened stars (Parthasarathy+, 1995) J/AJ/107/1433 : Cygnus OB2 polarimetry (Kobulnicky+, 1994) J/MNRAS/298/753 : Variables in Cygnus OB2 (Pigulski+ 1998) Associations, stellar Photometry, CCD Photometry, UBV The galactic association Cygnus OB2, which contains heavily reddened O and B stars, has been studied using CCD UBV photometry and spectroscopy. The file "mt91.dat" contains precise coordinates, UBV photometry, and spectral types from the study of Cygnus OB2, and merges the tables 2, 5 and 6 from the paper.
Observations in Cyg OB2 (tables 2,5,6) MT91 ? Star identification number=1 the first two stars in the list were outside the MT91 survey area, but new spectral types for them were given in Table 6. The positions for these 2 stars come from the ACT and GSC v1.2, and agree with those in the table to within an arcsecond or so. --- RAh Right Ascension J2000 (hours) number=2 positions were computed from original x,y by Brian Skiff, see the "History" section below h RAm Right Ascension J2000 (minutes) number=2 positions were computed from original x,y by Brian Skiff, see the "History" section below min RAs Right Ascension J2000 (seconds) number=2 positions were computed from original x,y by Brian Skiff, see the "History" section below s DE- Declination J2000 (sign) number=2 positions were computed from original x,y by Brian Skiff, see the "History" section below --- DEd Declination J2000 (degrees) number=2 positions were computed from original x,y by Brian Skiff, see the "History" section below deg DEm Declination J2000 (minutes) number=2 positions were computed from original x,y by Brian Skiff, see the "History" section below arcmin DEs Declination J2000 (seconds) number=2 positions were computed from original x,y by Brian Skiff, see the "History" section below arcsec Vmag V magnitude mag U-B U-B colour derived from B-V mag u_U-B Uncertainty flag on U-B number=3 the colon ':' indicates a uncertainty greater than 2-sigma, and the question mark '?' an error greater than 3-sigma (these were given as a double colon in the source paper) --- B-V B-V colour mag u_B-V Uncertainty flag on B-V number=3 the colon ':' indicates a uncertainty greater than 2-sigma, and the question mark '?' an error greater than 3-sigma (these were given as a double colon in the source paper) --- SpType MK Spectral type number=4 only the MK spectral type determined by Massey & Thompson is listed here; types from other sources cited in the original tables were ignored. --- Rem Remarks number=5 The Remarks column shows those stars that were blended ('bl') in Massey & Thompson's analysis, and 'traditional' Schulte numbers (see 1956ApJ...124..530S) indicated in the MT91 tables (e.g. S 12). --- Brian Skiff Lowell Obs. Francois Ochsenbein CDS 1998 Sep 17 UNKNOWN UNKNOWN An electronic copy of Table 2 was prepared by Jean-Claude Mermilliod (Jean-Claude.Mermilliod@obs.unige.ch). The star positions were computed by Brian Skiff (bas@lowell.Lowell.Edu) from about 50 stars scattered across the four CCD fields, for which coordinates were found from the ACT or GSC version 1.2, plus a few faint stars from USNO-A1.0, with rms residuals of 0".6. UNKNOWN UNKNOWN Nomenclature Notes: The acronym "MT" is sometimes used to designate the stars from this list in the literature. MT91 should be preferred. J_AJ_101_1408.xml CCD observations of Abell clusters. V. Isophotometry of 175 brightest elliptical galaxies in Abell clusters J/AJ/101/1561 J/AJ/101/1561 Isophotometry of 175 Brt. Ell. Gal. in Abell Clus. CCD observations of Abell clusters. V. Isophotometry of 175 brightest elliptical galaxies in Abell clusters A C Porter D P Schneider J G Hoessel Astron. J. 101 1561 1991 1991AJ....101.1561P galaxies: clusters: general galaxies: elliptical and lenticular, cD galaxies: isophotometry Profiles of major- and minor-axis surface brightness, ellipticity, position angle, and isophote centroid are presently derived from isophotometry for a sample of 175 brightest cluster ellipticals (BCEs). The BCEs' average ellipticity is a sharply rising function of metric radius; less than a fourth of the sample exhibits significant ellipticity decrease with increasing radius. While at radii of less than 16 kpc the BCEs are rounder than the average elliptical, they become too flattened at radii greater than 30 kpc to represent a randomly-oriented oblate-spheroid population. These results indicate that BCE outer regions are dynamically strongly coupled to their either prolate or stringy clusters.
isophotometry of BCE NGC 'N' denotes that the following number is of NGC; in other case (' '), is of Abell --- ABELL Abell cluster number * If NGC='N' then NGC number --- Z redshift of the BCE --- SEEING FWHM of the seeing in the CCD image arcsec E4 ellipticity for semimajor axis of 4 kpc * Blank space means the BCE was not observed at that radius, or the isophoto was discarded (see paper p1576r) --- E16 above of 16 kpc --- E64 above of 64 kpc --- PA4 position angle of the major-axis of 4 kpc (see E4 above) deg PA16 above of 16 kpc deg PA64 above of 64 kpc deg decr_E if ellipticity decreasing outwards anywhere in its profile: e" = 2nd outward derivative of E, ~ = nearly equal, cpx = complex --- const_E 'Y' denotes constant ellipticity --- TWIST 'Y' denotes significant isophoto twisting --- ASYM 'Y' denotes significant asymmetry --- tb1.tex TeX file of Table 1 macro.tex macro file for tb1.tex Koichi Nakajima CDS 1993 Dec 07 UNKNOWN UNKNOWN The catalogue was provided by courtesy of A.C.Porter to H. Andernach; it was numbered A152 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 16-Apr-1994: First archived. (The date of the latest archiving, see the date of each file.) UNKNOWN UNKNOWN * The original file is in TeX form with a macro file. Conversion from TeX to ASCII form is made by H.Andernach. * The number of entries of table1 is 176 because a cD galaxy NGC4874 is included after the brightest cluster elliptical of A1656 (see paper p1576). * "BCE" stands for "brightest cluster elliptical(s)". J_AJ_101_1561.xml The young Magellanic cluster NGC 2004 J/AJ/102/137 J/AJ/102/137 NGC 2004 The young Magellanic cluster NGC 2004 D Bencivenni E Brocato R Buonanno V Castellani Astron. J. 102 137 1991 1991AJ....102..137B Clusters, galaxy Galaxies, nearby Photometry, BV The results of a new CCD photometric investigation of stars in the field of the LMC cluster NGC 2004 are reported and discussed. B, V photometry is given for more than 1500 objects, the large majority to be ascribed to the cluster. A new color-magnitude diagram is presented. It shows a well-defined blue sequence (BS) of H-burning stars, running from V~=21mag up to V~=13mag, together with a group of cluster He-burning red supergiants with V~=13mag and a clump of field red giants at about V~=19 mag. Theoretical evolutionary computations are reported covering the range of massive stars evolving in the cluster. These evolutionary tracks can match the observed CM diagram provided that a low efficiency of the surface convection (a low value of the mixing length) is adopted. Comparison of the theoretical luminosity function with the upper portion of the observed BS distribution suggests a cluster age of about 8 million years, in agreement with previous evaluations. The completeness of the sample and the contribution of field stars have been estimated. The CM distribution of cluster stars has been compared with the results of synthetic clusters based on the adopted evolutionary scenario. We find that the observed distribution of cluster stars in the different evolutionary phases appears in good agreement with prediction based on theoretical evolutionary lifetimes. Moreover, the distribution of H-burning stars agrees with a Salpeter distribution in the whole range 2<=M/M_{sun}_<=20. After a short review of the current theoretical scenario concerning massive stars, the CM diagram of field stars is discussed, reaching the conclusion that the observed clump of red giants is the natural consequence of the peculiar large lifetimes in the central He burning phase of stars with M~=3M_{sun}_.
Program stars magnitudes, colors and positions No Star identification number --- Vmag V magnitude mag B-V B-V colour mag X X position pix Y Y position pix Patricia Bauer CDS 1994 Dec 09 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_102_137.xml Radio properties of extragalactic IRAS sources J/AJ/102/1663 J/AJ/102/1663 Radio properties of extragal. IRAS sources Radio properties of extragalactic IRAS sources J J Condon J J Broderick Astron. J. 102 1663 1991 1991AJ....102.1663C II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989) Giovanelli and Haynes 1984, A.J., 89, 1. Helou et al., 1985, Ap.J.Lett., 298, L11. Helou and Walker, 1988, IRAS Catalogs and Atlases: Small Scale Structure Catalog (U.S. GPO, Washington, DC). (Cat. <VII/73>) Kron and Shane 1976, Ap&SS, 39, 401. Moshir et al., 1989, Explanatory Supplement to the IRAS Faint Source Survey (Jet Propulsion Laboratory, Pasadena). (Cat. <II/156>) Nilson 1973, Uppsala General Catalogue of Galaxies (Uppsala Astronomical Observatory, Uppsala). (Cat. <VII/26>) Sandage and Tammann 1981, A Revised Shapley-Ames Catalog of Bright Galaxies (Carnegie Institute of Washington, Washington, DC) (RSA). (Cat.<VII/51>) Veron-Cetty and Veron 1989, A Catalogue of Quasars and Active Nuclei, 4th edition (European Southern Observatory, Garching. Galaxies, IR Galaxies, radio Infrared sources Radio sources This catalog presents radio and optical identifications of extragalactic IRAS sources from the IRAS Faint Source Catalog |b| > 50{deg} (Moshir et al., 1989 Cat. <II/156>). Sources with flux density > 0.2 at 60 microns and with S_60_ > S_12_ were identified by position coincidence with radio sources stronger than 25 mJy and lying north of declination = 5{deg} on the Green Bank 4.85 GHz sky map. Published VLA maps, new 4.86 GHz VLA maps made with 15 arcsec resolution, and accurate optical positions were used to confirm 122 candidate identifications. This catalog contains a merged version of tables 1 and 2 from the paper.
Radio Properties of Extragalactic IRAS Sources (5.5{deg}.. Dec ..66{deg}) IRAS Name of source (IRAS Faint Source Catalog) number=1 The "IRAS" column gives the IRAS Faint Source Catalog name in the format FHHMM.M+DDMM, where the letter F signifies that it is from the FSC, and the last digit of the RA field being the integer part of the RA seconds (i.e. the IAU-style truncation). The 'Oname' columns gives an alternative name for the source, if any, taken from such catalogs as NGC, 3C, IC, and UGC. --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec l_S12 '<' if flux density is an upper limit --- S12 12 micron flux density number=2 These columns give flux density information at 12, 25, 60, and 100 microns. Flags preceding the flux densities indicate which flux densities are upper limits (indicated by a greater-than symbol in this column). Flux densities (in Jy) are taken from (in order or preference): IRAS Catalog of Large Optical Galaxies (Rice et al., 1988ApJS...68...91R Cat. <VII/109>), revised IRAS Bright Catalog Sample (Soifer et al., 1989AJ.....98..766S) IRAS Small Scale Structures Catalog (Helou and Walker, 1988)(Cat. <VII/73>) IRAS Faint Source Catalog, ver. 1 (Moshir et al., 1989) (Cat. <II/156>) Jy l_S25 '<' if flux density is an upper limit --- S25 25 micron flux density number=2 These columns give flux density information at 12, 25, 60, and 100 microns. Flags preceding the flux densities indicate which flux densities are upper limits (indicated by a greater-than symbol in this column). Flux densities (in Jy) are taken from (in order or preference): IRAS Catalog of Large Optical Galaxies (Rice et al., 1988ApJS...68...91R Cat. <VII/109>), revised IRAS Bright Catalog Sample (Soifer et al., 1989AJ.....98..766S) IRAS Small Scale Structures Catalog (Helou and Walker, 1988)(Cat. <VII/73>) IRAS Faint Source Catalog, ver. 1 (Moshir et al., 1989) (Cat. <II/156>) Jy S60 60 micron flux density number=2 These columns give flux density information at 12, 25, 60, and 100 microns. Flags preceding the flux densities indicate which flux densities are upper limits (indicated by a greater-than symbol in this column). Flux densities (in Jy) are taken from (in order or preference): IRAS Catalog of Large Optical Galaxies (Rice et al., 1988ApJS...68...91R Cat. <VII/109>), revised IRAS Bright Catalog Sample (Soifer et al., 1989AJ.....98..766S) IRAS Small Scale Structures Catalog (Helou and Walker, 1988)(Cat. <VII/73>) IRAS Faint Source Catalog, ver. 1 (Moshir et al., 1989) (Cat. <II/156>) Jy l_S100 '<' if flux density is an upper limit --- S100 100 micron flux density number=2 These columns give flux density information at 12, 25, 60, and 100 microns. Flags preceding the flux densities indicate which flux densities are upper limits (indicated by a greater-than symbol in this column). Flux densities (in Jy) are taken from (in order or preference): IRAS Catalog of Large Optical Galaxies (Rice et al., 1988ApJS...68...91R Cat. <VII/109>), revised IRAS Bright Catalog Sample (Soifer et al., 1989AJ.....98..766S) IRAS Small Scale Structures Catalog (Helou and Walker, 1988)(Cat. <VII/73>) IRAS Faint Source Catalog, ver. 1 (Moshir et al., 1989) (Cat. <II/156>) Jy RArh Radio Right Ascension (B1950) (hour) number=3 These columns give the B1950 radio position. All of these positions were measured with the VLA at 1.49 or 4.86 GHz, and their rms uncertainties are normally < 1 arcsec in each coordinate. Sources which are flagged with an asterisk in the rad_flg column are precise to 0.01s in RA and 0.1" in Dec. Sources which are not flagged are precise to 0.1s in RA and 1" in Dec. h RArm Radio Right Ascension (B1950) (min) min RArs Radio Right Ascension (B1950) (sec) s DEr- Radio Declination sign (B1950) number=3 These columns give the B1950 radio position. All of these positions were measured with the VLA at 1.49 or 4.86 GHz, and their rms uncertainties are normally < 1 arcsec in each coordinate. Sources which are flagged with an asterisk in the rad_flg column are precise to 0.01s in RA and 0.1" in Dec. Sources which are not flagged are precise to 0.1s in RA and 1" in Dec. --- DErd Radio Declination (B1950) (deg) deg DErm Radio Declination (B1950) (arcmin) arcmin DErs Radio Declination (B1950) (arcsec) arcsec S4850 Flux density at 4850 MHz number=4 This column gives the Green Bank 4.85 GHz flux density (in mJy) from the 87GB Catalog (Gregory and Condon 1991ApJS...75.1011G, Cat.<VIII/14>) or the flux density as measured from the sky maps. mJy refs References to published VLA maps number=5 This column gives references to published VLA maps. Some of these papers contain additional references to published radio data: 1 Condon (1987ApJS...65..485C) or Condon et al. (1987ApJS...65..543C) 2 Condon et al. (1990ApJS...73..359C) 3 Condon et al. (1991AJ....101..362C) --- Oname Alternative name of source number=1 The "IRAS" column gives the IRAS Faint Source Catalog name in the format FHHMM.M+DDMM, where the letter F signifies that it is from the FSC, and the last digit of the RA field being the integer part of the RA seconds (i.e. the IAU-style truncation). The 'Oname' columns gives an alternative name for the source, if any, taken from such catalogs as NGC, 3C, IC, and UGC. --- RAoh Optical Right Ascension (B1950) (hour) number=6 These columns give the B1950 optical position Sources which are flagged with an asterisk in the 'opt_flg' column were measured with 0.5" rms accuracy (Condon et al., 1991AJ....101..362C or new measurements) and are precise to 0.01s in RA and 0.1" in Dec. Sources which are not flagged in the 'opt_flg' column were measured with 4" rms accuracy (Dressel and Condon 1976ApJS...31..187D; Condon and Broderick (1988AJ.....96...30C) Condon et al., 1991AJ....101..362C) and are precise to 0.1s in RA and 1" in Dec. h RAom Optical Right Ascension (B1950) (min) min RAos Optical Right Ascension (B1950) (sec) s DEo- Optical Declination sign (B1950) number=6 These columns give the B1950 optical position Sources which are flagged with an asterisk in the 'opt_flg' column were measured with 0.5" rms accuracy (Condon et al., 1991AJ....101..362C or new measurements) and are precise to 0.01s in RA and 0.1" in Dec. Sources which are not flagged in the 'opt_flg' column were measured with 4" rms accuracy (Dressel and Condon 1976ApJS...31..187D; Condon and Broderick (1988AJ.....96...30C) Condon et al., 1991AJ....101..362C) and are precise to 0.1s in RA and 1" in Dec. --- DEod Optical Declination (B1950) (deg) deg DEom Optical Declination (B1950) (arcmin) arcmin DEos Optical Declination (B1950) (arcsec) arcsec opt_flg '*' if higher accuracy in position number=6 These columns give the B1950 optical position Sources which are flagged with an asterisk in the 'opt_flg' column were measured with 0.5" rms accuracy (Condon et al., 1991AJ....101..362C or new measurements) and are precise to 0.01s in RA and 0.1" in Dec. Sources which are not flagged in the 'opt_flg' column were measured with 4" rms accuracy (Dressel and Condon 1976ApJS...31..187D; Condon and Broderick (1988AJ.....96...30C) Condon et al., 1991AJ....101..362C) and are precise to 0.1s in RA and 1" in Dec. --- type Optical type for UGC galaxies number=7 These columns give optical information on the identifications. The optical morphological type (type) is taken from Nilson (1973) for UGC galaxies. The apparent photographic magnitude (Pmag) has been corrected for Zwicky magnitude errors (Kron and Shane 1976) in the area between 7h and 18h, south of 15 {deg} (see Giovanelli and Haynes 1984). The distance (dist) is given in Mpc from the Revised Shaply-Ames Catalog (Sandage and Tammann 1981, Cat <VII/51>) or from Hubble distance based on Ho = 50 km/s/Mpc. The q column gives the FIR/radio flux-ratio parameter, defined by q = log( [ FIR / (3.75x10^12^ Hz) ] / S_4.85_ ) where S_4.85 is the 4.85 GHz flux density (W m^-2^ Hz^-1^) and FIR == 1.26x10^14^( 2.58*S_60_ + S_100_) is the total far-infrared flux (W m^-2^) between 42.5 and 122.5 microns obtained from the IRAS 60 micron and 100 micron flux densities (Jy) (Helou et al., 1985. (Cat. <VII/73>)) --- Pmag Apparent photographic magnitude number=7 These columns give optical information on the identifications. The optical morphological type (type) is taken from Nilson (1973) for UGC galaxies. The apparent photographic magnitude (Pmag) has been corrected for Zwicky magnitude errors (Kron and Shane 1976) in the area between 7h and 18h, south of 15 {deg} (see Giovanelli and Haynes 1984). The distance (dist) is given in Mpc from the Revised Shaply-Ames Catalog (Sandage and Tammann 1981, Cat <VII/51>) or from Hubble distance based on Ho = 50 km/s/Mpc. The q column gives the FIR/radio flux-ratio parameter, defined by q = log( [ FIR / (3.75x10^12^ Hz) ] / S_4.85_ ) where S_4.85 is the 4.85 GHz flux density (W m^-2^ Hz^-1^) and FIR == 1.26x10^14^( 2.58*S_60_ + S_100_) is the total far-infrared flux (W m^-2^) between 42.5 and 122.5 microns obtained from the IRAS 60 micron and 100 micron flux densities (Jy) (Helou et al., 1985. (Cat. <VII/73>)) --- dist Optical distance number=7 These columns give optical information on the identifications. The optical morphological type (type) is taken from Nilson (1973) for UGC galaxies. The apparent photographic magnitude (Pmag) has been corrected for Zwicky magnitude errors (Kron and Shane 1976) in the area between 7h and 18h, south of 15 {deg} (see Giovanelli and Haynes 1984). The distance (dist) is given in Mpc from the Revised Shaply-Ames Catalog (Sandage and Tammann 1981, Cat <VII/51>) or from Hubble distance based on Ho = 50 km/s/Mpc. The q column gives the FIR/radio flux-ratio parameter, defined by q = log( [ FIR / (3.75x10^12^ Hz) ] / S_4.85_ ) where S_4.85 is the 4.85 GHz flux density (W m^-2^ Hz^-1^) and FIR == 1.26x10^14^( 2.58*S_60_ + S_100_) is the total far-infrared flux (W m^-2^) between 42.5 and 122.5 microns obtained from the IRAS 60 micron and 100 micron flux densities (Jy) (Helou et al., 1985. (Cat. <VII/73>)) Mpc q FIR/radio flux-ratio parameter number=7 These columns give optical information on the identifications. The optical morphological type (type) is taken from Nilson (1973) for UGC galaxies. The apparent photographic magnitude (Pmag) has been corrected for Zwicky magnitude errors (Kron and Shane 1976) in the area between 7h and 18h, south of 15 {deg} (see Giovanelli and Haynes 1984). The distance (dist) is given in Mpc from the Revised Shaply-Ames Catalog (Sandage and Tammann 1981, Cat <VII/51>) or from Hubble distance based on Ho = 50 km/s/Mpc. The q column gives the FIR/radio flux-ratio parameter, defined by q = log( [ FIR / (3.75x10^12^ Hz) ] / S_4.85_ ) where S_4.85 is the 4.85 GHz flux density (W m^-2^ Hz^-1^) and FIR == 1.26x10^14^( 2.58*S_60_ + S_100_) is the total far-infrared flux (W m^-2^) between 42.5 and 122.5 microns obtained from the IRAS 60 micron and 100 micron flux densities (Jy) (Helou et al., 1985. (Cat. <VII/73>)) --- Sp-Index Radio spectral index between 1.4 and 5 GHz number=8 The alpha column gives the radio spectral index defined by alpha = -log(S1/S2)/log(nu1/nu2) where nu1 ~5 GHz and nu2 ~1.4 GHz. The values of S1 were taken from the S4850 column or from Condon et al., (1991AJ....101..362C). The values of S2 are based on the VLA maps in Condon (1987ApJS...65..485C), Condon and Broderick (1988AJ.....96...30C), Condon et al. (1990ApJS...73..359C) or Condon et al (1991AJ....101..362C) unless otherwise noted in the paper. The alphaIR column gives the FIR spectral index defined by alphaIR = log(S_60_/S_25_)/log(60/25) l_alphaIR is flagged with '>' if alphaIR is a lower limit. --- l_alphaIR '>' if alphaIR is a lower limit number=8 The alpha column gives the radio spectral index defined by alpha = -log(S1/S2)/log(nu1/nu2) where nu1 ~5 GHz and nu2 ~1.4 GHz. The values of S1 were taken from the S4850 column or from Condon et al., (1991AJ....101..362C). The values of S2 are based on the VLA maps in Condon (1987ApJS...65..485C), Condon and Broderick (1988AJ.....96...30C), Condon et al. (1990ApJS...73..359C) or Condon et al (1991AJ....101..362C) unless otherwise noted in the paper. The alphaIR column gives the FIR spectral index defined by alphaIR = log(S_60_/S_25_)/log(60/25) l_alphaIR is flagged with '>' if alphaIR is a lower limit. --- alphaIR Spectral index between 60 and 25 microns number=8 The alpha column gives the radio spectral index defined by alpha = -log(S1/S2)/log(nu1/nu2) where nu1 ~5 GHz and nu2 ~1.4 GHz. The values of S1 were taken from the S4850 column or from Condon et al., (1991AJ....101..362C). The values of S2 are based on the VLA maps in Condon (1987ApJS...65..485C), Condon and Broderick (1988AJ.....96...30C), Condon et al. (1990ApJS...73..359C) or Condon et al (1991AJ....101..362C) unless otherwise noted in the paper. The alphaIR column gives the FIR spectral index defined by alphaIR = log(S_60_/S_25_)/log(60/25) l_alphaIR is flagged with '>' if alphaIR is a lower limit. --- source Dominant radio energy source number=9 This column gives the dominant radio energy source: stars (S) or monster (M). --- notes '*' if there is a note on the src. number=10 This column is marked with an asterisk if there is a note on the source in the published paper. These notes are typically notes on UGC galaxies or the AGN spectral type classifications, and are taken from the compilation of Veron-Cetty and Veron (1989). --- Patricio Ortiz CDS 1999 Mar 29 UNKNOWN UNKNOWN "The catalogue was originally archived as A053 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_AJ_102_1663.xml BVR photoelectric sequences for selected fields in the Palomar Sky Survey and the magnitude-diameter relation J/AJ/102/395 J/AJ/102/395 BVR photoelectric sequences in the PSS BVR photoelectric sequences for selected fields in the Palomar Sky Survey and the magnitude-diameter relation R M Humphreys R Landau F D Ghigo W Zumach A E Labonte Astron. J. 102 395 1991 1991AJ....102..395H Photometry, BV BVR photoelectric photometry and positions are reported for 437 stars in 49 Palomar Sky Survey fields. A relation is derived between the Johnson BVR photometry and the E and O photographic magnitudes on the Palomar plates. The BVR photometry, the E and O magnitudes, and the 1950 positions are presented in the accompanying catalog.
Catalog of BVR photometric sequences Star The Sky Survey field number and number of the star within the field number=1 The finding chart for each object is identified by the same sequence number --- Vmag V magnitude mag e_Vmag Error on V mag mag B-V B-V colour index mag e_B-V Error on B-V colour index mag V-R V-R colour index mag e_V-R Error on V-R colour index mag Nobs Number of observations --- Emag Derived E magnitude on the POSS (Palomar Observatory Sky Survey) as explained in the paper mag e_Emag Error on E magnitude mag Omag Derived O magnitude on the POSS as explained in the paper mag e_Omag Error on O magnitude mag RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec pmRA Proper motion in right ascension arcsec/yr pmDE Proper motion in declination arcsec/yr Marie-Jose Wagner, Simona Mei CDS 1995 Apr 21 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_102_395.xml The Stellar Content of LH 9 and 10 (N 11) in the LMC: A Case for Sequential Star Formation J/AJ/103/1205 J/AJ/103/1205 Stellar Content of LH 9 and 10 in the LMC The Stellar Content of LH 9 and 10 (N 11) in the LMC: A Case for Sequential Star Formation J W Parker C D Garmany P Massey N R Walborn Astron. J. 103 1205 1992 1992AJ....103.1205P Magellanic Clouds Photometry, UBV We present CCD photometry and spectroscopy for stars in Lucke-Hodge 9 and 10, two adjacent OB association in the northwest corner of the LMC. Our catalog contains UBV photometry (complete to ~18min in all three filters) for 795 stars and BV-only photometry (complete to ~19min in both filters) for an additional 434 stars.
UBV data from Tables 3-6 in the paper Star Star number number=1 Stars with numbers <3000 are in LH 9, and numbers >3000 are in LH 10. Star numbers 1001 through 1522 are from Table 3. Star numbers 2001 through 2345 are from Table 4. Star numbers 3001 through 3273 are from Table 5. Star numbers 4001 through 4089 are from Table 6. --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Xpos X position number=2 Since the CCD frames for these fields (LH 9 and 10) are not contiguous, the X and Y coordinates refer to different coordinate systems for LH 9 and LH10; for orientation of the coordinate systems see the CCD finder charts in the article. Pixel sizes (in X and Y columns) are approximately 0.49 arcsec/pixel. pix Ypos Y position number=2 Since the CCD frames for these fields (LH 9 and 10) are not contiguous, the X and Y coordinates refer to different coordinate systems for LH 9 and LH10; for orientation of the coordinate systems see the CCD finder charts in the article. Pixel sizes (in X and Y columns) are approximately 0.49 arcsec/pixel. pix Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag e_Vmag Error on V magnitude mag e_B-V Error on B-V colour mag e_U-B Error on U-B colour mag All stars with UBV photometry with their bolometric magnitudes and effective temperatures which were not listed in the original tables. Star Star number number=1 Stars numbers 1001 through 1522 are located in LH 9 (Table 10), and 3001 through 3273 in LH 10 (Table 11). In the journal article, Tables 10 and 11 listed the Bluest (Q<-0.7) and Brightest (V<16) Stars in LH 9 and 10, and Table 12 listed other stars with known spectral types. The table here contains ALL stars with UBV photometry (e.g., all stars that are listed in Tables 3 and 5), and includes their bolometric magnitudes and effective temperatures which were not listed in the original tables. --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Xpos X position number=2 Since these fields are not contiguous, the X,Y coordinates refer to different coordinate systems: they are from the CCD finder charts in the article. Pixel sizes are approximately 0.49 arcsec/pixel. pix Ypos Y position number=2 Since these fields are not contiguous, the X,Y coordinates refer to different coordinate systems: they are from the CCD finder charts in the article. Pixel sizes are approximately 0.49 arcsec/pixel. pix Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag Q (U-B)-0.72(B-V) mag E(B-V) Color excess calculated from Q or spectral type or mean reddening as discussed in Section 3.1 of the article. mag Mv Absolute V magnitude=V-Rv*E(B-V)-DM where Rv=3.1, and the distance modulus DM=18.3 mag mag log(Teff) log10 of the effective temperature: is calculated from Q or (B-V)0 as discussed in Section 3.2 of the article. K Mbol Bolometric magnitude=Mv+BC, where BC is calculated from Teff as discussed in Section 3.2 of the article. mag Sp Spectral type and luminosity class as determined from spectroscopic observations number=3 One colon ":" indicates an uncertainty of one spectral subtype or luminosity class, and two colons "::" indicate a larger uncertainty. --- Comments Comments number=4 Comments in square brackets, [], are indicated by the following codes (note that these codes are somewhat different than those that appear in the original paper): [a]: strong Balmer lines [b]: possible composite / blend; spectrum contaminated by nearby star (in some cases the number of the other star is given in parentheses) [c]: cosmic ray hits / bad pixels [d]: weak Balmer lines [e]: strong nebular emission in the Balmer lines [g]: weak N lines [p]: Star 3264 is a ZAMS star with extremely strong nebular emission lines and is located in the compact HII knot N 11A (see text) [z]: ZAMS O star --- Simona Mei CDS 1995 Apr 04 Joel Wm. Parker <joel.parker@gsfc.nasa.gov> J_AJ_103_1205.xml A Photometric Study of the "Second Parameter" Globular Cluster Palomar 14 J/AJ/103/131 J/AJ/103/131 Photometric Study of Globular Palomar 14 A Photometric Study of the "Second Parameter" Globular Cluster Palomar 14 S Holland W E Harris Astrophys. Journ. 103, No. 1 131 1992 1992AJ....103..131H Clusters, globular Colors Photometry, UBV This catalog contains relative coordinates and deep B and V CCD photometry for 327 stars in a field of the second-parameter outermost-halo globular cluster Palomar 14. It corresponds to Table 3 in the published source reference. It is based on six V and four B frames obtained with the RCA4 CCD camera at the prime focus of the 3.6m CFHT on May 16-17 1988. The resultant limiting V magnitude is approximately 24.5. The scale factor is 0.206 arcsec/pixel. Positions are given in the table as "x" and "y" in pixel units, where x increases Eastward and y increases Southward. The star identification numbers given by the authors are arbitrary and were assigned in order of increasing y. The V magnitudes and the (B-V) colors are tabulated. The data reduction was done using DAOPHOT . Palomar 14 is located at R.A.=16h08.8m and Dec=+15deg,05.2min (1950). The field observed is centered approximately 1.14' West and 2.32' South of the cluster center.
The catalogue Ident Star identification --- x x coordinate (+x=E; 1 pixel= 0.206") pixel y y coordinate (+y=S; 1 pixel= 0.206") pixel V V magnitude mag (B-V) (B-V) color mag J.E. Gass Hughes STX/NASA 1995 Sep 08 UNKNOWN UNKNOWN Machine-readable version records were sorted in order of ascending star identifier as submitted by author. The published table was printed in order of decreasing V magnitude. ReadMe by J. E. Gass (Hughes STX) Sep. 1995. J_AJ_103_131.xml A search for stars of very low metal abundance. II. J/AJ/103/1987 J/AJ/103/1987 A search for stars of very low metal abundance. II. A search for stars of very low metal abundance. II. T C Beers G W Preston S A Shectman Astron. J. 103 1987 1992 1992AJ....103.1987B Equivalent widths Radial velocities Stars, metal-deficient Spectroscopic observations for 1044 stars located primarily in the southern Galactic hemisphere are reported; the stars were chosen from a list of candidate metal-deficient stars discovered in the HK objective-prism survey. Radial velocities and line indices based on the equivalent widths of Ca II, K, H-gamma and H-delta, and the CH G band are reported. Estimates of metallicity for 874 stars with derived abundances less than -0.5 are presented.
Observational data, derived distances, and abundances Star Star Identification --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg V V magnitude mag B-V B-V color mag U-B U-B color mag E(B-V) B-V excess mag BV BV color estimate, obtained from calibration of Balmer Index HP mag RV Radial velocity km/s Det Detector Identification: R = Reticon; F = 2D-Frutti; R/F = both --- KP CaII K equivalent width index KP (Angstroms) 0.1nm HP Balmer line equivalent width index HP (Angs.) 0.1nm GP G-band equivalent width index GP (Angstroms) 0.1nm Type Classification of stellar type --- Mv Absolute magnitude estimate mag Dist Distance estimate (kpc) kpc Wk Interstellar CaII K estimate (as in Beers 1990, AJ 99, 323) --- [Fe/H]k estimate from Norris models --- [Fe/H]c adopted estimate --- Note on duplicity number=1 List of known duplicates: CS 22173- 2 = CS 30494- 4 CS 22173- 7 = CS 30494- 20 CS 22173- 14 = CS 30494- 15 CS 22173- 15 = CS 30494- 40 CS 22173- 21 = CS 30494- 33 CS 22886- 8 = CS 29512- 6 CS 22886- 12 = CS 29512- 15 CS 22886- 13 = CS 29512- 13 CS 22886- 22 = CS 29512- 18 CS 22886- 29 = CS 29512- 27 CS 22886- 42 = CS 29512- 51 CS 22888- 14 = CS 30493- 23 CS 22888- 39 = CS 30493- 56 CS 22937- 34 = CS 30492- 56 CS 22937- 42 = CS 30492- 76 CS 22937- 72 = CS 30492-102 = CS 29501- 51 CS 22937- 73 = CS 29501- 52 CS 29513- 16 = CS 30493- 74 --- Francois Ochsenbein CDS 1993 May 04 J_AJ_103_1987.xml Spectroscopy of hot stars in the galactic halo J/AJ/103/267 J/AJ/103/267 Spectroscopy of hot stars in the galactic halo Spectroscopy of hot stars in the galactic halo T C Beers G W Preston S A Shectman S P Doinidis K E Griffin Astron. J. 103 267 1992 1992AJ....103..267B Spectroscopy Stars, early-type Spectroscopy for 769 hot stars from the HK objective-prism/ interference-filter survey of Beers et al. (1985) is presented. 193 of these stars also have broadband UBV colors available. When available, photometric information is used to obtain estimates of the surface temperature for degenerates and for O- and B-type subdwarfs, based on previously derived calibrations. Several extremely hot (T(eff) greater than 50,000 K) He-rich sdO stars are identified.
Results (tables 4a to 4e) Star Star Identification --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) . DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg V magnitude mag B-V color mag U-B color mag E(B-V) B-V excess mag RV Heliocentric Radial velocity km/s Det Detector Identification: R = Reticon; F = 2D-Frutti --- HP Balmer line equivalent width index HP (A) 0.1nm D0.2 H-delta breadth D(0.2) at 20% below local continuum (Angstroms) 0.1nm Rc Line depth of H-delta (Rc) relative to local continuum 0.1nm KP CaII K equivalent width index KP (Angstroms) 0.1nm HeI4026 Equivalent width of HeI 4026 (Angstroms) 0.1nm HeI4387 Equivalent width of HeI 4387 (Angstroms) 0.1nm HeI4471 Equivalent width of HeI 4471 (Angstroms) 0.1nm Table Flag indicating in the original table: a: Degenerate Stars b: Subdwarf O and B Stars c: FHB, A, and FHB/A Stars d: Composite Stars e: Narrow-lined B Stars --- Class Classification of stellar type from objective-prism spectrum --- Type Stellar type from digital spectrum and photometry --- logTeff Estimate of Log Teff K Note "D" for Duplicated star --- Francois Ochsenbein CDS 1993 May 04 UNKNOWN UNKNOWN Duplicated stars: CS 22169- 1 = CS 22190- 9 CS 22173- 1 = CS 30494- 1 CS 22173- 24 = CS 30494- 32 CS 22173- 33 = CS 30494- 50 CS 22875- 2 = CS 22881- 69 CS 22886- 32 = CS 29512- 44 CS 22888- 17 = CS 30493- 27 (Note: Radial velocities are different) CS 22897-112 = CS 22956- 6 (Note: Radial velocities are different) CS 22937- 22 = CS 30492- 42 CS 22937- 36 = CS 30492- 62 CS 22937- 82 = CS 30492-118 CS 22937- 17 = CS 30492- 29 CS 22937- 65 = CS 30492- 98 CS 22937- 25 = CS 30492- 46 (Note: Radial velocities are different) CS 22937- 87 = CS 30492-126 (Note: Radial velocities are different) J_AJ_103_267.xml Deep CCD photometry and variable stars in the metal-rich globular cluster M 71 J/AJ/103/460 J/AJ/103/460 CCD photometry of M 71 Deep CCD photometry and variable stars in the metal-rich globular cluster M 71 P J C Hodder J M Nemec H B Richer G G Fahlman Astron. J. 103 460 1992 1992AJ....103..460H Clusters, globular Stars, variable Two sets of observations of the metal-rich globular cluster M 71 are presented. The first uses deep CCD exposures to derive a fiducial in V, B-V and compares this with a cluster of similar metallicity, 47 Tuc. Comparison with oxygen enhanced theoretical isochrones leads to age estimates for M 71 of from ~14+/-2Gyr to ~16+/-2Gyr. Within the limits imposed by the quality of the data, no significant age difference between the two clusters is found. The second set of 73 frames is used to search an overlapping 67"x104" area of the cluster for variable stars. Light curves and phase diagrams (where appropriate) are presented for all four of the variables discovered. One variable blue straggler (or SX Phe star) has been identified with a period of 0.050d. Values for its mass depend, of course, on the assumed pulsation mode-(0.90+/-0.47)M_{sun}_ for the first overtone mode, and (1.57+/-0.83)M_{sun}_ for the fundamental mode. One of the variables, with a 0.0582d period, but with a magnitude 1.75mag below the main sequence turnoff may be a field star. Two candidate eclipsing binary systems were also found. The most likely orbital period of one is 0.372d. This value, and the shape of the light curve, suggest that it could be a W UMa type variable. No period was obtainable for the other candidate binary due to a lack of phase coverage. Further data is needed to confirm and strengthen these claims, and to check for cluster membership.
Photometry of M71 ID Identification number --- Cud A '*' indicates Cudworth stars that have a cluster membership probability of 50% or more --- n_ID Note on the stars number=1 Name of the variables discussed in section 4. --- X X position pix Y Y position pix Vmag V magnitude mag B-V B-V colour mag U-B U-B colour mag Marie-Jose Wagner, Patricia Bauer CDS 1994 Dec 05 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_103_460.xml Stellar occultation candidates from the Guide Star Catalog. I. Saturn, 1991-1999 J/AJ/103/983 J/AJ/103/983 Stellar occultation candidates of Saturn Stellar occultation candidates from the Guide Star Catalog. I. Saturn, 1991-1999 A S Bosh S W Mcdonald Astron. J. 103 983 1992 1992AJ....103..983B Occultations Solar system We present a list of 203 potential occultations by Saturn and its rings of stars from the Hubble Space Telescope Guide Star Catalog (GSC), during the years 1991-1999. Because the GSC is not a complete catalog, this is not an exhaustive list of Saturn occultations. In particular, stars brighter than magnitude 8 are not included. However, this list does include many fainter candidates than do current occultation candidate lists for Saturn; these fainter stars also can provide a high signal-to-noise ratio if observed with a large telescope or in the infrared where Saturn and its rings have absorption bands. We list the occultation circumstances, as well as star information found in the GSC.
Saturn occultation candidates: Geocentric circumstances for closet approach GSC GSC star number --- Date Predicted date of closest approach "DD/MM/YY" UTh Predicted time of closest approach (hours) h UTm Predicted time of closest approach (min) min Dist Distance between the star and Saturn at closest approach arcsec n_Dist Note on distance number=1 * : These events are nominal hits. The star is within Saturn or its rings (as indicated in the last column) by less than 2.2arcseconds. **: These events are nominal misses. The star is outside Saturn or its rings by less than 2.2 arcseconds. --- PA Position angle deg Mag Magnitude mag n_Mag Note on magnitude number=2 t: Magnitude is approximately V. --- Vel Velocity km/s SunEl Solar elongation angle deg RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Plate GSC plate number --- EastLong East longitude on Earth of the sub-Saturn point deg Event Type of event number=3 S: occultation by Saturn R: occultation by its rings --- James Marcout, Patricia Bauer CDS 1995 Feb 14 UNKNOWN UNKNOWN Keypunched at CDS * 14-Feb-1995: first archived at CDS * 15-May-1995: three errors corrected in table1 J_AJ_103_983.xml Infrared-luminous giants in M32: an intermediate-age population? J/AJ/104/1349 J/AJ/104/1349 Infrared-luminous giants in M32 Infrared-luminous giants in M32: an intermediate-age population? W L Freedman Astron. J. 104 1349 1992 1992AJ....104.1349F Galaxies, nearby Photometry, infrared Stars, luminous A previously unknown population of very luminous, red, asymptotic-giant-branch stars has been identified as a result of near-infrared (JHK) imaging in the dwarf elliptical galaxy M32. Situated above the tip of the normal first red giant branch, these stars are intrinsically brighter than the most luminous normal giants in old Galactic globular clusters by approximately 2 bolometric magnitudes. Moreover, they are a full bolometric magnitude brighter than the brightest giants observed in our own Galactic bulge. Several possible explanations for this population are examined, including old long-period variables, binary mergers, supermetallicity, and intermediate-age stars. It is suggested that the simplest explanation at present, is that M32 had a star formation episode less than about 5 billion years ago. These stars would then be the evolved extended asymptotic giant branch population resulting from that event (similar to those stars observed in the intermediate-age clusters in the Magellanic Clouds). This population may be similar to that in the M31 bulge, recently observed by Rich and Mould. The detection of a young component in M32 is of particular interest because historically, M32 has been a fiducial galaxy for population synthesis techniques. An understanding of M32 remains crucial for our understanding of distant and more luminous elliptical galaxies.
M32 JK photometry Id Star identification number --- Xpos X position pix Ypos Y position pix Kmag K magnitude mag Jmag J magnitude mag J-K J-K colour mag James Marcout, Patricia Bauer CDS 1995 Feb 23 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_104_1349.xml Canada-France-Hawaii Telescope blue grens quasar candidates J/AJ/104/1706 J/AJ/104/1706 CFH Telescope Blue Grens Quasar Candidates Canada-France-Hawaii Telescope blue grens quasar candidates D Crampton A P Cowley F D A Hartwick P W Ko Astron. J. 104 1706 1992 1992AJ....104.1706C quasars: general Positions and magnitudes are given for 488 quasar candidates, 14 compact emission-line galaxies, and eight white dwarf candidates discovered with Canada-France-Hawaii blue grens in a 7.5 square degree area in the directions 1338 + 27 and 1639 + 40. The goal of this survey is to enlarge the areas previously surveyed in these regions to provide magnitude-limited samples of quasars for the study of the luminosity function and large scale distribution of quasars at moderate to high redshifts. Redshifts are given for seven of the new quasars, including one BAL quasar. Note: The explanations for last three columns are not clear in the present paper, and those found in Crampton et al. 1985 (AJ, 90, 987) p994 are adopted.
1338+27 field candidates 1639+40 field candidates NAMEra the RA part of IAU (1986) name --- NAMEde the DE part of IAU (1986) name --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign . DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec Mb estimated blue magnitude mag Q category code (see paper p1707, and also the previous paper, AJ,90,987, p994) --- REM 'R'= a remark is given in "notes2" or "notes3", respectively --- Koichi Nakajima CDS 1993 Dec 07 UNKNOWN UNKNOWN The catalogue was provided by courtesy of D.Crampton to H. Andernach; it was numbered A155 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 16-Apr-1994: First archived. (The date of the latest archiving, see the date of each file.) J_AJ_104_1706.xml Galactic structure from faint Stroemgren photometry: the catalog of observations J/AJ/104/1765 J/AJ/104/1765 Faint Stroemgren photometry Galactic structure from faint Stroemgren photometry: the catalog of observations T A von Hippel Astron. J. 104 1765 1992 1992AJ....104.1765V Photometry, uvby We have initiated a faint photometric survey in the Stroemgren system covering ~1 square degree and including 1238 objects in order to develop samples which best probe the thick disk population. The catalog of observations are presented here. They were acquired without kinematic or metallicity biases and are complete to V=17.3-18.5, depending on the field, for 810 early to relatively late type (K0 V or G5 III) stars. Photometric metallicities were derived for 508 stars and indicate a metal-poor stellar population, consistent with a mixture of thick disk and halo stars. While the Stroemgren u-band was not part of the survey, follow-up u-band observations of 32 survey objects indicate that intermediate color survey stars (0.3<=b-y<=0.5) are main-sequence or slightly evolved stars, while redder survey stars (b- y>=0.5) are giants. The survey catalog is available in electronic form upon request.
Stroemgren survey photometry Field Field number --- Id Identification number in the field --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vmag Apparent V magnitude mag b-y b-y colour index mag v-b v-b colour index mag e_vmag rms uncertainty on v magnitude mag o_vmag Number of observations in v magnitude --- e_bmag rms uncertainty on b magnitude mag o_bmag Number of observations in b magnitude --- e_ymag rms uncertainty on y magnitude mag o_ymag Number of observations in y magnitude --- uvby observations Field Field number --- --- --- Id Identification number in the field --- Vmag V magnitude mag b-y b-y colour index mag v-b v-b colour index mag u-v u-v colour index mag e_ymag rms uncertainty on ymag mag e_bmag rms uncertainty on bmag mag e_vmag rms uncertainty on vmag mag e_umag rms uncertainty on umag mag James Marcout, Patricia Bauer CDS 1997 May 16 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_104_1765.xml Structure, rotation, and the peculiar velocity cD galaxy in Abell 2107 J/AJ/104/2078 J/AJ/104/2078 Galaxies in Abell 2107 Field Structure, rotation, and the peculiar velocity cD galaxy in Abell 2107 W R Oegerle J M Hill Astron. J. 104 2078 1992 1992AJ....104.2078O Galaxies Radial velocities As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.
Velocity data ID Identifying number --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DEd Declination J2000 deg DEm Declination J2000 arcmin DES Declination J2000 arcsec cz Observed heliocentric-corrected velocity km/s Com Comments on the presence of emission lines and the galaxies used as correlation templates --- Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_104_2078.xml Homogeneous JHKL photometry of a sample of BL Lac Objects J/AJ/104/28 J/AJ/104/28 Homogeneous JHKL photometry of BL Lac Objects Homogeneous JHKL photometry of a sample of BL Lac Objects M Bersanelli P Bouchet R Falomo E G Tanzi Astron. J. 104 28 1992 1992AJ....104...28B BL Lac objects Photometry, infrared Homogeneous J, H, K, L, photometry of 42 BL Lacertae objects is presented. The observations cover a period of 3 yr with a typical time interval of 6 months.
Program Objects Name BL Lac name --- z Redshift --- Av Absorption mag X/R X or Radio flag --- Comments Comments --- Ref References number=1 References to Table 1 1. Feigelson et al. (1986) 2. Wardle, Moore and Angel (1984) 3. Fosbury and Disney (1976) 4. Carswell et al. (1974) 5. Gioia et al. (1984) 6. Disney, Peterson and Rodgers (1974) 7. Bowyer, Brodie, Clarke, and Henry (1984) 8. Falomo et al (1991) 9. Smith et al (1988) 10. Falomo and Treves (1990) 11. Falomo et al. (1987) 12. Falomo et al. (1988) 13. Tanzi et al. (1986) 14. Worrall et al. (1984) 15. Tapia et al. (1977) 16. Bregman et al. (1984) 17. Wall et al. (1986) 18. Filippenko et al. (1986) 19. Ulmer et al. (1983) 20. Falomo et al. (1989) 21. Ledden and O'Dell (1985) 22. Nicolson et al. (1979) 23. Fricke et al. (1983) 24. Landau et al. (1986) 25. Falomo (1991a) 26. Stocke et al. (1982) 27. Stickel et al. (1991) 28. Brissenden et al (1990) 29. Stickel et al (1988) 30. Falomo and Tanzi (1991) 31. Halpern et al (1991) 32. Falomo (1991b) 33. Falomo (1990) 34. Peterson et al. (1973) 35. Owen and Mufson (1977) 36. Condon et al (1977) 37. Bolton et al (1975) 38. Ulrich (1981) 39. Bolton and Wall (1970) 40. Bolton et al (1975) 41. Bolton et al (1966) 42. Remillard et al (1989) --- JHKL Fluxes Name BL Lac name --- MJD Modified Julian Date JD J Flux in filter mJy e_J mean error on J mJy H Flux in filter mJy e_H mean error on H mJy K Flux in filter mJy e_K mean error on K mJy L Flux in filter mJy e_L mean error on L mJy Spectral indices Name BL Lac name number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component --- Note Notes (see below) number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component --- amean spectral index (F proportional (nu)**(-a) number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component --- Nobs Number of observations number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component --- amin Minimal value of spectral index number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component --- e_amin mean error on amin number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component --- amax Maximal value of spectral index number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component --- e_amax mean error on amax number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component --- pcGal Fractional estimated flux contribution of the host galaxy to the observed spectrum. number= a) Near a bright star b) Significant positive curvature c) Spectral index is derived after subtraction of the thermal component % Francois Ochsenbein CDS 1993 Mar 19 J_AJ_104_28.xml Triton stellar occultation candidates 1992-1994 J/AJ/104/862 J/AJ/104/862 Stellar occultation candidates Triton stellar occultation candidates 1992-1994 S W McDonald J L Elliot Astron. J. 104 862 1992 1992AJ....104..862M Occultations Positional data A search for Triton stellar occultation candidates for the period 1992-1994 has been completed with CCD strip-scanning observations. The search reached an R magnitude of about 17.4 and found 129 candidates within 1.5arcsec of Triton's ephemeris during this period. Of these events, we expect around 30 occultations to be visible from the Earth, indicating that a number of Triton occultation events should be visible from major observatories. Even the faintest of our candidate events could produce useful occultation data if observed with a large enough telescope. Our astrometric accuracy is inadequate to identify which of these appulse events will produce occultations on the Earth; further astrometry is needed to refine the predictions for positive occultation identification. To aid in selecting candidates for additional astrometric and photometric studies, we include finder charts and Earth-based visibility charts for each event.
Possible occultations by Triton ID Star name --- AppDate Date of the closest approach "DD/MM/YY" Apph UT time of the closest approach h Appm UT time of the closest approach min SepMin Minimum separation of the closest approach arcsec PA Position angle of Triton relative to the star at the time of the closest approach deg Rmag CCD magnitude mag Vel Shadow velocity km/s Dist Angular distance between Triton and the Sun deg RAh Right ascension (J2000) of the star h RAm Right ascension (J2000) of the star min RAs Right ascension (J2000) of the star s DE- Declination sign --- DEd Declination (J2000) of the star number=1 The declination is also the sub-Earth latitude of the star. deg DEm Declination (J2000) of the star number=1 The declination is also the sub-Earth latitude of the star. arcmin DEs Declination (J2000) of the star number=1 The declination is also the sub-Earth latitude of the star. arcsec GLON Sub-Earth longitude of the star deg Strip Strip numbers on which an image of the candidate star was measured --- James Marcout, Patricia Bauer CDS 1995 May 10 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_104_862.xml The HII Regions of the Galaxy M101 J/AJ/104/92 J/AJ/104/92 HII Regions Properties in M101 The HII Regions of the Galaxy M101 P A Scowen R J Dufour J J Hester Astron. J. 104 92 1992 1992AJ....104...92S Abundances Galaxies, nearby Galaxies, optical HII regions Interstellar matter Spectrophotometrically calibrated CCD imagery of two overlapping 16 arc min fields in the SAB(rs)cdI galaxy M101 in the emission of H alpha, [O III] lambda 5007, H beta, and [S II] lambda 6723 are used to study various physical properties of the H II region population. Individual H II regions are identified and mapped using an automated algorithm, thus eliminating personal bias in the measurements. Characteristics of the population studied include the H II region luminosity function and radial variations in extinction, [O III]/H beta, O/H, [S II]/H alpha, ionization parameter, and numbers of ionizing photons. In addition, radial and azimuthal variations in the H II surface density are studied in comparision to that of H I and H_2 inferred from radio 21 cm and CO observations. It is demonstrated that the magnitude of trends and ``gradients'' found from such analyses depend on the surface brightness threshold set in defining the H II region boundaries; so results are presented for both low (log S(H alpha) = -15.7 ergs s^-1 cm^-2 arcsec^-2; 625 H II regions) and high (-15.0; 248 H II regions) thresholds. Radial gradients in both extinction, C(H beta), and O/H are seen in the H II region population -- with a distinct flattening in the O/H gradient seen in the outer disk beginning at about 10 kpc. The luminosity function of the H II region population found is similar to previous studies, though both the high and low ends are sensitive to the threshold levels set. Other parameters, such as the ionization parameters, luminosities, and size distribution, show no evidence for systematic variations with galactocentric distance. Current star formation processes active in the disk of M101 are analyzed two-dimensionally by comparison of the distribution of ionized and neutral hydrogen. The star formation efficiency shows considerable variation across the disk, suggesting significant spatial variation in the critical density for cloud collapse across the disk of M101 and thus departures from the simple Toomre model.
Table of derived properties of HII regions used in Figures 3,4,5,6 and 7. Higher threshold used. [Rnum,CHb,O3Hb,S2Ha,OH,U,Q] Rnum HII Region Reference Number --- CHb Balmer Decrement as C(H beta) --- O3Hb Ratio of [O III] to H beta --- S2Ha Ratio of [S II] to H alpha --- OH Oxygen Abundance as 12+log(O/H) --- U Ionization Parameter --- Q Number of Ionizing photons /s 10+45ct/s Table of observed properties of HII regions used in paper. Not explicitly presented in paper - see last paragraph of Summary section in paper. [Rnum,RAh,RAm,RAs,DEd,DEm,DEs,A, Ha,Hb,O3,S2,Rad] Rnum HII Region Reference Number --- RAh Region RA Hour (1950.0) h RAm Region RA Minute (1950.0) min RAs Region RA Second (1950.0) s DE- Sign of declination --- DEd Region Dec Degree (1950.0) deg DEm Region Dec Minute (1950.0) arcmin DEs Region Dec Second (1950.0) arcsec A Region Area, 1 pix = 1.2 arcsec pix2 Ha H alpha surf.brightness, 1pix=1.2" mW/m2/pix Hb H beta surf.brightness, 1pix=1.2" mW/m2/pix O3 surf.brightness, [OIII], 1pix=1.2" mW/m2/pix S2 surf.brightness, [S II], 1pix=1.2" mW/m2/pix Rad Radial distance of region in galaxy pc Paul A. Scowen Arizona State Univ. 1995 Jan 17 J_AJ_104_92.xml Photometric calibration of the HST Wide-Field/Planetary Camera. II. Ground-based observations of calibration fields J/AJ/105/1196 J/AJ/105/1196 HST WF/PC photometric calibration Photometric calibration of the HST Wide-Field/Planetary Camera. II. Ground-based observations of calibration fields H C Harris D A Hunter W A Baum J H Jones Astron. J. 105 1196 1993 1993AJ....105.1196H Photometry Ground-based CCD observations have been made simulating the photometric properties of the Wide-Field/Planetary Camera (WF/PC) of the Hubble Space Telescope. This paper gives results in 15 of the most important WF/PC passbands for two fields chosen to provide efficient in-flight calibration of the WF/PC. These calibration fields are located in the outskirts of the globular clusters Omega Cen and NGC 6752.
WF/PC flight calibration standards in Omega Cen WF/PC flight calibration standards in NGC 6752 ID Star number from identification in fig. 3 for table1 and fig. 4 for table2 --- RAh Right ascension 2000 h RAm Right ascension 2000 min RAs Right ascension 2000 s DE- Declination sign --- DEd Declination 2000 deg DEm Declination 2000 arcmin DEs Declination 2000 arcsec F336W F336W magnitude mag F439W F439W magnitude mag F547M F547M magnitude mag F555W F555W magnitude mag F569W F569W magnitude mag F606W F606W magnitude mag F622W F622W magnitude mag F675W F675W magnitude mag F702W F702W magnitude mag F791W F791W magnitude mag F814W F814W magnitude mag F725LP F725LP magnitude mag F785LP F785LP magnitude mag F850LP F850LP magnitude mag F1042M F1042M magnitude mag e_F336W rms uncertainty on F336W mag e_F439W rms uncertainty on F439W mag e_F547M rms uncertainty on F547M mag e_F555W rms uncertainty on F555W mag e_F569W rms uncertainty on F569W mag e_F606W rms uncertainty on F606W mag e_F622W rms uncertainty on F622W mag e_F675W rms uncertainty on F675W mag e_F702W rms uncertainty on F702W mag e_F791W rms uncertainty on F791W mag e_F814W rms uncertainty on F814W mag e_F725LP rms uncertainty on F725LP mag e_F785LP rms uncertainty on F785LP mag e_F850LP rms uncertainty on F850LP mag e_F1042M rms uncertainty on F1042M mag ci_F336W Crowding index for F336W --- o_F336W Number of observations for F336W --- ci_F439W Crowding index for F439W --- o_F439W Number of observations for F439W --- ci_F547M Crowding index for F547M --- o_F547M Number of observations for F547M --- ci_F555W Crowding index for F555W --- o_F555W Number of observations for F555W --- ci_F569W Crowding index for F569W --- o_F569W Number of observations for F569W --- ci_F606W Crowding index for F606W --- o_F606W Number of observations for F606W --- ci_F622W Crowding index for F622W --- o_F622W Number of observations for F622W --- ci_F675W Crowding index for F675W --- o_F675W Number of observations for F675W --- ci_F702W Crowding index for F702W --- o_F702W Number of observations for F702W --- ci_F791W Crowding index for F791W --- o_F791W Number of observations for F791W --- ci_F814W Crowding index for F814W --- o_F814W Number of observations for F814W --- ci_F725LP Crowding index for F725LP --- o_F725LP Number of observations for F725LP --- ci_F785LP Crowding index for F785LP --- o_F785LP Number of observations for F785LP --- ci_F850LP Crowding index for F850LP --- o_F850LP Number of observations for F850LP --- ci_F1042M Crowding index for F1042M --- o_F1042M Number of observations for F1042M --- Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_1196.xml A survey of the Pisces-Perseus supercluster. V. The declination strip +33.5 deg to +39.5 deg and the main supercluster ridge J/AJ/105/1251 J/AJ/105/1251 Velocities in Pisces-Perseus supercluster. A survey of the Pisces-Perseus supercluster. V. The declination strip +33.5 deg to +39.5 deg and the main supercluster ridge G Wegner M P Haynes R Giovanelli Astron. J. 105 1251 1993 1993AJ....105.1251W J/A+AS/130/341 : Groups of Galaxies in PPS (Trasarti-Battistoni 1998) Dressel, L. L., & Condon, J. J. 1976, ApJS, 31, 187 (1976ApJS...31..187D) Haynes, M. P., & Giovanelli, R. 1984, AJ, 89, 758 (HG84) (1984AJ.....89..758H) Haynes, M. P., Giovanelli, R., Starosta, B., & Magri, C. A., 1988, AJ, 95, 607 (1988AJ.....95..607H) Hewitt, J. N., Haynes, M. P., & Giovanelli, R. 1983, AJ, 88, 272 (1983AJ.....88..272H) Magri, C. A. 1990, Ph.D. thesis, Cornell University Nilson, P. 1973, in Uppsala General Catalog, Uppsala Astron. Obs. Ann. 6 (UGC, See Cat. <VII/26>) Zwicky, F., Herzog, E., Karpowicz, M., Kowal, C. T., & Wild, P. 1961-1968, Catalogue of Galaxies and Clusters of Galaxies (California Institute of Technology, Pasadena), Vols. 1-6 (CGCG, see cat. <VII/190>) Clusters, galaxy Combined data Galaxies, optical H I data Radial velocities Redshifts Measurements of 544 radial velocities, 229 optical and 315 in the 21cm HI line, are presented for galaxies, mostly in the declination strip +33.5 deg<Dec<+39.5deg in the region of the Pisces-Perseus supercluster. These are combined with other available data to investigate the linear structure identified as the main supercluster ridge. The main ridge of the supercluster extends at least 50h^-1Mpc before it disappears into the zone of avoidance east of Perseus. Confinement both on the plane of the sky and in the velocity dimension imply an axial ratio of greater than ten to one and an inclination with respect to the plane of the sky of less than about 12 degrees. The smoothed volume density contrast over the whole ridge averages more than a factor of 6 relative to the average density derived for the whole sample. The relative proximity, low inclination to the plane of the sky, and high contrast relative to the foreground and background, help to make the Pisces-Perseus filament one of the most prominent features in the extragalactic sky on large scales.
Galaxies with new optical redshifts CGCG Identification in the Catalog of Galaxies and Clusters of Galaxies (Zwicky et al. 1961-68 (CGCG)), that is the field number and then the entry number within that field --- UGC Uppsala General Catalog (UGC) entry number (Nilson 1973) --- n_NGC/IC New General Catalogue (NGC) or Index Catalog (IC) indicator, 'N' or 'I', respectively --- NGC/IC NGC/IC number --- RAh Right ascension 1950 number=1 For galaxies brighter than m=14.5, positions were obtained from Dressel & Condon (1976). For others, coordinates were obtained from the CGCG or, when higher accuracy than that of the CGCG is manifest, they were obtained from the Palomar Sky Survey (PSS) prints using a standard overlay program, with an estimated accuracy of 10". h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec T Morphological type code index number=2 Morphological type code index: 0 - Elliptical 1 - SO 3 - Sa 5 - Sb 7 - Sc 9 - Irregular 10 - Peculiar, with intermediate types allowed. A "B" indicates the presence of a bar. --- a Major diameter from the UGC where available or else measured by eye from the PSS prints arcmin b Minor diameter arcmin i Inclination derived from the axial ratio following Haynes & Giovanelli (HG84). deg m(z) Magnitude given in the CGCG or the UGC. mag m(c) Corrected magnitude, after applying the corrections for galactic and internal extinction, redshift and systematic effects as discussed by HG84. mag RV Heliocentric velocity km/s e_RV Standard deviation on RV number=3 For emission line-derived redshifts, the standard deviation of the mean for all the lines measured, or +/-60 km/s, which is the estimated error for a single line in this sample. For absorption line-derived redshifts, errors are estimated from the JKFOUR program, to a minimum acceptable value of +/-25 km/s. km/s n_RV Spectral features used for RV number=4 A simple indicator of whether the spectral features used to derive the redshift were seen in emission (e) or absorption (a). For a handful of galaxies, velocities were derived from two absorption line spectra (x) and combining both absorption and emission lines (y). --- V(0) Local Group velocity, assuming a correction for the Sun's motion of 300 sin l cos b, where l and b are the galactic longitude and latitude. km/s log(L) Luminosity, h^2^L, derived from m(c) and V(0). [solLum] Parameters of objects observed at 21 cm CGCG Identification in the Catalog of Galaxies and Clusters of Galaxies (Zwicky et al. 1961-68 (CGCG)), that is the field number and then the entry number within that field --- UGC Uppsala General Catalog (UGC) entry number (Nilson 1973) --- m_UGC UGC component designation --- n_NGC/IC New General Catalogue (NGC) or Index Catalog (IC) indicator, 'N' or 'I', respectively --- NGC/IC NGC/IC number --- RAh Right ascension 1950 number=1 For galaxies brighter than m=14.5, positions were obtained from Dressel & Condon (1976). For others, coordinates were obtained from the CGCG or, when higher accuracy than that of the CGCG is manifest, they were obtained from the Palomar Sky Survey (PSS) prints using a standard overlay program, with an estimated accuracy of 10". h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec T Morphological type code index number=2 Morphological type code index: 0 - Elliptical 1 - SO 3 - Sa 5 - Sb 7 - Sc 9 - Irregular 10 - Peculiar, with intermediate types allowed. A "B" indicates the presence of a bar. --- a Major diameter from the UGC where available or else measured by eye from the PSS prints arcmin b Minor diameter arcmin i Inclination derived from the axial ratio following Haynes & Giovanelli (HG84). deg m(z) Magnitude given in the CGCG or the UGC. mag m(c) Corrected magnitude, after applying the corrections for galactic and internal extinction, redshift and systematic effects as discussed by HG84. mag RV 21 cm line heliocentric velocity number=6 RV measured as the midpoint of the emission profile at a level of 50% of the mean signal intensity. When the object was considered to be undetected at 21 cm (Q=0), the velocity corresponds to the frequency of the central channel of the spectrometer km/s V(0) Adopted Local Group velocity number=7 Adopted Local Group velocity, assuming a correction for the Sun's motion of 300 sin l cos b, where l and b are the galactic longitude and latitude. The adopted heliocentric velocity is the 21 cm velocity if the object is a high quality detection; if not, the optical velocity is adopted, when available. km/s W1 Observed 21 cm profile width, measured at a level of 50% of the mean signal intensity. km/s W2 Observed 21 cm profile width, measured at a level of 20% of the peak signal intensity. km/s Wc 21 cm profile width corrected for viewing inclination and to the rest frame of the observer km/s Fobs Observed 21 cm line flux Jy.km/s Fc 21 cm line flux, after correction for pointing, beam dilution, and internal absorption following HG84. Jy.km/s NWc rms noise in baseline 21 cm line profile, where available. mJy snr Signal-to-noise ratio of HI emission spectrum, measured as the ratio of peak signal flux to e_Wc, where available. --- log(L) Logarithm of optical luminosity, log10(h^2 L), with h = H0/100 km/s/Mpc. [solLum] log(M_H_) Logarithm of HI mass , log10(h^2 M(H)). [solMass] Tel Telescope identification code for HI observations number=3 Telescope identification code: 0 - Arecibo 305 m with dual circular feed 1 - Green Bank 91 m 2 - Effelsberg 100 m B - Arecibo 305 m with linear feed major axis mapping. --- Q Quality code for HI detection number=4 Quality code: 0 - Object considered to be undetected at 21 cm. 21 cm line observations were performed, so we list the rms noise per channel of the observations. But no signal was detected; hence no flux is given. 1 - High quality detection 2 - Marginal to poor detection 3 - Flux and velocity ok, but profile unsuitable for use in T-F relation 4 - HI seen in absorption 5 - Confused with neighbor --- Ref Reference code for HI data number=5 The HI data reported here come from one of the following sources: 1 - This survey 2 - Northern Pisces-Perseus region (Haynes et al. 1988) 3 - Isolated galaxy survey (HG84) 4 - Survey of large angular diameter galaxies (Hewitt et al. 1983) 5 - Magri (1990) 6 - Sc galaxy survey (in preparation) --- Note Note flag (see file notes2.dat) --- Notes to table2 Galaxy Galaxy name, either CGCG or U followed by UGC number, repeated if note spans on lines. --- Text Text of Note --- table1.tex LaTeX version of table1 table2.tex LaTeX version of table2 notes2.tex LaTeX version of notes2 Patricia Bauer CDS 1994 Jun 20 UNKNOWN UNKNOWN * 20-Jun-1994: From AAS CD-ROM series, Volume 1, 1993, ReadMe adapted * 01-Mar-1999: ReadMe revisited at CDS J_AJ_105_1251.xml A survey of the Pisces-Perseus supercluster. VI. The declination zone +15.5 deg to +21.5 deg J/AJ/105/1271 J/AJ/105/1271 Pisces-Perseus supercluster. VI A survey of the Pisces-Perseus supercluster. VI. The declination zone +15.5 deg to +21.5 deg R Giovanelli M P Haynes Astron. J. 105 1271 1993 1993AJ....105.1271G J/A+AS/130/341 : Groups of Galaxies in PPS (Trasarti-Battistoni 1998) Haynes, M. P., & Giovanelli, R. 1984, AJ, 89, 758 (HG84) (1984AJ.....89..758H) Hewitt, J. N., Haynes, M. P., & Giovanelli, R. 1983, AJ, 88, 272 (1983AJ.....88..272H) Karachentsev, I. 1989, AJ, 97, 1566 (1989AJ.....97.1566K) Magri, C. A. 1990, Ph.D. thesis, Cornell University Nilson, P. 1973, in Uppsala General Catalog, Uppsala Astron. Obs. Ann. 6 (UGC, See Cat. <VII/26>) Zwicky, F., Herzog, E., Karpowicz, M., Kowal, C. T., & Wild, P. 1961-1968, Catalogue of Galaxies and Clusters of Galaxies (California Institute of Technology, Pasadena), Vols. 1-6 (CGCG, see cat. <VII/190>) Clusters, galaxy H I data New results are presented of Arecibo observations in the 21 cm line of 765 galaxies with declinations between 15.5 deg and 21.5 deg, in the Pisces-Perseus supercluster zone. If considered independently on the neighboring parts of the sky, this region, to the South of the supercluster ridge, shows significantly less evidence of structure on large scales in excess of 30 Mpc, contrasting substantially with the characteristics of the declination zones immediately to the North.
Parameters of observed objects CGCG Identification in the Catalog of Galaxies and Clusters of Galaxies (Zwicky et al. 1961-68: (CGCG)), that is the field number followed by the entry number within that field --- UGC Uppsala General Catalog (UGC) entry number (Nilson 1973) --- m_UGC UGC component designation --- n_NGC/IC New General Catalogue (NGC) or Index Catalog (IC) indicator, 'N' or 'I', respectively --- NGC/IC NGC/IC number --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec T Morphological type code index number=1 Morphological type code index: 0 - Elliptical 1 - SO 3 - Sa 5 - Sb 7 - Sc 9 - Irregular 10 - Peculiar 12 - Generic spiral (S...) 13 - Compact, unresolved morphology 14 - Compact spiral or irregular, with intermediate types allowed A "B" indicates the presence of a bar. --- a Major diameter from the UGC where available or else measured by eye from the PSS prints arcmin b Minor diameter arcmin i Inclination derived from the axial ratio following Haynes & Giovanelli (HG84). deg m(z) Magnitude given in the CGCG or the UGC. mag m(c) Corrected magnitude, after applying the corrections for galactic and internal extinction, redshift and systematic effects as discussed by HG84. mag RV 21 cm line heliocentric velocity, measured as the midpoint of the emission profile at a level of 50% of the mean signal intensity. km/s V(0) Adopted Local Group velocity number=5 Adopted Local Group velocity, assuming a correction for the Sun's motion of 300 sin l cos b, where l and b are the galactic longitude and latitude. The adopted heliocentric velocity is the 21 cm velocity if the object is detected When the object was considered to be undetected at 21 cm (Q=0), the velocity corresponds to the frequency of the central channel of the spectrometer km/s W1 Observed 21 cm profile width, measured at a level of 50% of the mean signal intensity. km/s W2 Observed 21 cm profile width, measured at a level of 20% of the peak signal intensity. km/s Wc 21 cm profile width corrected for viewing inclination and for redshift broadening km/s Fobs Observed 21 cm line flux integral Jy.km/s Fc 21 cm line flux integral, after correction for random pointing errors, beam dilution, and HI internal absorption following HG84. Jy.km/s Sigma rms noise per channel measured in signal and interference-free portions of the spectrum mJy snr Signal-to-noise parameter of HI emission spectrum, measured as the ratio of peak signal flux to rms noise, after smoothing. --- log(L) Logarithm of optical luminosity, log10(h^2 L), derived from m(c) and scaled by the dimensionless Hubble parameter, h = H0/100 km/s/Mpc. [solLum] log(M_H_) Logarithm of HI mass , log10(h^2 M(H)). derived from Fc and V(0). [solMass] Tel Telescope identification code for HI observations number=2 Telescope identification code: 0 - Arecibo 305 m with dual circular feed 1 - 300-foot telescope at Green Bank 7 - Arecibo 305 m with flat (linear polarization) feed --- Q Quality code for HI detection number=3 Quality code: 0 - Object considered to be undetected at 21 cm. 21 cm line observations were performed, so we list the rms noise per channel of the observations. But no signal was detected; hence no flux is given. 1 - High quality detection 2 - Marginal to poor detection 3 - Flux and velocity ok, but profile unsuitable for use in T-F relation 4 - HI seen in absorption 5 - Confused with neighbor --- Ref Reference code for HI data. number=4 The HI data reported here come from one of the following sources: 1 - This survey 2 - Isolated galaxy survey (HG84) 3 - Survey of large angular diameter galaxies (Hewitt et al. 1983) 4 - Galaxy observed by the authors and I. Karachentsev as part of the thin galaxy survey based on the catalog of Karachentsev (1989); visual magnitude estimate on PSS. 5 - Not explained in the article --- Note Note flag (see file notes1.dat) --- Notes to table1 Galaxy Galaxy name, either CGCG or U followed by UGC number, repeated if note spans on lines. --- Text Text of Note --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1994 Jun 21 UNKNOWN UNKNOWN * 20-Jun-1994: From AAS CD-ROM series, Volume 1, 1993, ReadMe adapted * 01-Mar-1999: ReadMe revisited at CDS J_AJ_105_1271.xml The open cluster IC 4665 J/AJ/105/1441 J/AJ/105/1441 The open cluster IC 4665 The open cluster IC 4665 C F Prosser Astron. J. 105 1441 1993 1993AJ....105.1441P Clusters, open Photometry Proper motions The results of a combined astrometric, photometric, and spectroscopic program to identify members of the open cluster IC 4665 are presented. Numerous new proper motion/photometric candidate members and at least 23 M dwarfs with H-alpha emission have been identified.
IC 4665: Lick 30 s plates (3 exposures, each of 30 s duration) proper motion candidates IC 4665: Yerkes & Lick proper motion candidates P Running identification number --- V Johnson V magnitude mag B-V B-V color mag V-I V-I color mag R-I R-I color mag v Number of observations at V magnitude --- b Number of observations at B magnitude --- i Number of observations at I magnitude --- r Number of observations at R magnitude --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec X Survey coordinates (East) mm Y Survey coordinates (North) mm pmX Relative proper motion component arcsec/100yr pmY Relative proper motion component arcsec/100yr e_pmX Error in pmX, one-sigma error arcsec/100yr e_pmY Error in pmY, one-sigma error arcsec/100yr PROB Proper motion membership probability number=1 A proper motion membership probability has been determined from gaussian fitting to the cluster and field proper motion distributions - however the reader is advised not to attach great weight to the probabilities calculated due to the high contamination of field stars found for this cluster. No proper motion membership probabilities were calculated for the Lick candidates in table2 due to the rough approximations made to correct for magnitude dependent effects in the proper motions during the analysis of the Lick 30min/1hr plate reductions. --- N Number of Yerkes fields used to determine proper motion (table2 only) --- Member Membership on the basis of photometry --- Other Other previous identifications --- Patricia Bauer CDS 1994 Jun 21 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_1441.xml U. S. Naval Observatory photographic parallaxes. List IX J/AJ/105/1571 J/AJ/105/1571 U. S. Naval Observatory photographic parallaxes U. S. Naval Observatory photographic parallaxes. List IX R S Harrington C C Dahn V V Kallarakal H H Guetter B Y Riepe R L Walker J R Pier F J Vrba C B Luginbuhl H C Harris H D Ables Astron. J. 105 1571 1993 1993AJ....105.1571H Parallaxes, trigonometric Photometry, UBV Proper motions Trigonometric parallaxes, relative proper motions, and photometry are presented for 122 stars in 111 systems. Of these stars, 70 are brighter than V = 10.0.
Astrometric and photometric results No USNO running number --- Name Star name --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign ('N' for north, 'S' for south) --- DEd Declination J2000 deg DEm Declination J2000 arcmin CD Emulsion/filter code (CD; see end of notes1.dat; blank means see notes for details) --- Plates Number of plates --- DeltaT Time interval --- plx Relative parallax arcsec e_plx Standard error in relative parallax arcsec pm Magnitude of proper motion (J2000) arcsec/yr e_pm Standard error in proper motion magnitude arcsec/yr pa Direction of proper motion (J2000) deg e_pa Standard error in proper motion direction deg plxAbs Estimated absolute parallax arcsec e_plxAbs Standard error in estimated absolute parallax arcsec V V magnitude mag e_V Standard error in V, bright (V < 10) star photometric errors are all less than 0.01, unless indicated in the notes, and are not given in the table. mag B-V B-V color mag e_B-V Standard error in B-V mag U-B U-B color mag e_U-B Standard error in U-B mag O_UBV Number of photometric observations and the number of U-B observations if different. An "#" means the quoted value is taken from the literature, and is indicated in the notes. Blank means see the notes. --- M Absolute visual magnitude mag e_M Standard error in absolute visual magnitude mag Vel Tangential velocity km/s e_Vel Standard error in tangential velocity km/s References star positions and parallax star aliases NO USNO running number --- Star Star name --- Ref. Reference star positions, measured in arcseconds eastward and northward from the target star, and some alternative designations --- Patricia Bauer CDS 1994 Jun 21 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_1571.xml The morphological catalogue of galaxies equatorial survey J/AJ/105/1637 J/AJ/105/1637 The morphological catalogue of galaxies equatorial The morphological catalogue of galaxies equatorial survey J Huchra D W Latham L N Da Costa P S Pellegrini C N A Willmer Astron. J. 105 1637 1993 1993AJ....105.1637H Galaxies Redshifts We present 865 redshifts of galaxies located in the equatorial strip -17.5 deg <= Dec. <= -2.5 deg in the right ascension range 20 h <= R.A. <= 5 h. Redshifts have been obtained for the complete sample of all 833 galaxies in the Morphological Catalog of Galaxies with magnitudes brighter than m = 14.5 (corresponding approximately to m(Zwicky) = 15.0). This sample also includes three galaxies from other sources with more reliable magnitudes, satisfying this limit, and 29 fainter galaxies, usually companions of the galaxies in the magnitude limited sample.
Radial velocities Radial velocities Name Name of the galaxy adopting the order NGC, IC, or coordinates as suggested by the IAU --- RAh Right ascension 1950.0, from the Morphological Catalog of Galaxies (MCG). Occasionally these can be greatly in error and better positions were adopted whenever possible. h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950.0 from MCG deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec m(B) Magnitude, m(B) from MCG, of the galaxy. Especially for brighter galaxies, more accurate magnitudes were taken from other sources, even though they are not exactly on the same photometric system (see notes1 file) mag Source Source of magnitude (see notes1 file) --- RV Heliocentric velocity km/s e_RV Heliocentric velocity error km/s r_RV Velocity source (see notes1 file ) --- T de Vaucouleurs' morphological types. Additional types (beyond de Vaucouleurs' range) are from the CfA Redshift Catalog (Huchra et al. 1992, available from the NSSDC and CDS), e.g., type "20" is a "Spiral galaxy" that has not been subclassified further. --- d1 Major diameter arcmin d2 Minor diameter arcmin MCG MCG (or Markarian or Zwicky) name --- tables.tex TeX version of the tables Patricia Bauer CDS 1994 Jun 21 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_1637.xml The metallicity gradient and distribution function of globular clusters around NGC 1399 J/AJ/105/1762 J/AJ/105/1762 The metallicity gradient and distribution function The metallicity gradient and distribution function of globular clusters around NGC 1399 P Ostrov D Geisle J C Forte Astron. J. 105 1762 1993 1993AJ....105.1762O Galaxies Photometry, CMT1T2V We have obtained integrated Washington photometry (C,M,T1) of globular cluster candidates in the field of NGC 1399. This galaxy, the dominant object in the Fornax cluster, shares with NGC 4486 (M87) the property of possessing one of the largest known specific frequencies of globulars. Conflicting evidence on the presence of a B-V color gradient as a function of galactocentric distance has been reported for this cluster system. Here we investigate the existence of a gradient using the C-T1 index, which is twice as metallicity sensitive as B-V.
Washington Photometry of globular cluster candidates in NGC 1399 n_ID Field identification Central field = 0, north field = 1 south field = 2 and west field = 3 --- ID Running ID number --- X X coordinate pix Y Y coordinate pix C-M C-M color mag M-T1 M-T1 color mag T1 T1 magnitude mag e_C-M Error in C-M mag e_M-T1 Error in M-T1 mag e_T1 Error in T1 mag Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_1762.xml Proper motions, membership, and photometry of open clusters near eta Carinae J/AJ/105/1822 J/AJ/105/1822 Proper motions, membership, and photometry of Proper motions, membership, and photometry of open clusters near eta Carinae K M Cudworth S C Martin K Degioia-Eastwood Astron. J. 105 1822 1993 1993AJ....105.1822C Clusters, open Photometry, photographic Proper motions Proper motions and photographic photometry have been derived for nearly 600 stars with 7.5 < V < 15.5 in the region of the very young open clusters Tr 14, Tr 16, and Cr 232 based on 26 plates dating from 1893 to 1990.
Positions, proper motions, photometry, and membership probabilities Name Star identification number FA: Feinstein et al. (1973) FB: Feinstein (1982) HD: Henry Draper Catalogue Y: This study --- X X coordinate number=1 X, Y positions are given in a coordinate system that is aligned with right ascension and declination of equator and equinox 1950, but positions are epoch 1975. The zero point of these offsets is star Y1 (V=12.82) which lies at 10:42:32.87 -59:20:29.0 (equator and equinox 1950) arcsec Y Y coordinate number=1 X, Y positions are given in a coordinate system that is aligned with right ascension and declination of equator and equinox 1950, but positions are epoch 1975. The zero point of these offsets is star Y1 (V=12.82) which lies at 10:42:32.87 -59:20:29.0 (equator and equinox 1950) arcsec pmX Relative proper motion in X 10-5arcsec/yr e_pmX rms uncertainty on pmX 10-5arcsec/yr pmY Relative proper motion on Y 10-5arcsec/yr e_pmY rms uncertainty on pmY 10-5arcsec/yr V V magnitude mag B-V B-V color mag Member Calculated membership probability % Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_1822.xml A model of the 2-35 micron point source infrared sky J/AJ/105/1860 J/AJ/105/1860 2-35 micron point source IR sky model A model of the 2-35 micron point source infrared sky M Cohen Astron. J. 105 1860 1993 1993AJ....105.1860C Models Photometry, infrared The Point Source Infrared Sky Model of Wainscoat et al. [ApJS, 83, 111 (1992)] is extended to make predictions for any filter lying wholly within the range 2.0 to 35.0 microns. The development of a library of complete 2-35micron low-resolution spectra (with 0.1micron step size) that represent the 87 categories of Galactic object and four types of extragalactic source implicit in the Model supports this extension. This library is based upon the "spectral template" technique whereby existing spectral fragments for individual sources (from ground-based, airborne, and satellite-borne instruments) are combined into complete spectra. Templates provide a natural way to represent the complete spectral energy distributions of celestial sources for which only infrared photometry and/or partial spectroscopy are available. Consequently, templates bear upon the important general problem of establishing midinfrared calibration sources. The new Model is validated by comparison with broadband K (2.2micron) source counts.
Model categories of source Cat Category --- Source Source/LRS? number=1 An asterisk, "*", preceding an object name indicates that an IRAS Low Resolution Spectrometer (LRS) spectrum is not available for that source. Source names surrounded by braces, "{}", denote sources whose spectra were not used in the creation of the average template for their category. --- Rtot Total range for the infrared spectral information available um Ref References for the spectral fragments --- Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_1860.xml Photometry of dwarf K and M stars J/AJ/105/1962 J/AJ/105/1962 K and M stars photometry Photometry of dwarf K and M stars E W Weis Astron. J. 105 1962 1993 1993AJ....105.1962W Photometry, UBVRI Stars, dwarfs Stars, late-type Broadband UBVRI photometry is presented for 687 stars from among the dwarf K and M stars found spectroscopically by Vyssotsky [AJ, 63, 211 (1958)]. Of these, 211 are without previous photometry.
Photometry of Vyssotsky stars VYSS Vyssotsky number number=1 References: Vyssotsky A.N., 1943 AJ, 97, 381 (First list) Vyssotsky A.N., Janssen E.M., Miller W.J. & Walther M.E., ApJ 104, 234 (Second list) Vyssotsky A.N. & Mateer B.A., ApJ 116, 117 (Third list) Vyssotsky A.N., 1956 AJ 61, 201 (Fourth list) Vyssotsky A.N., 1958 AJ, 63, 211 (Supplement list) --- m_VYSS Letters designating components of multiple star systems --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEmin Declination 1950 arcmin V V magnitude mag u_V uncertainty flag on V --- B-V B-V color mag u_B-V uncertainty flag on B-V --- U-B U-B color mag u_U-B uncertainty flag on U-B --- V-R V-R color mag u_V-R uncertainty flag on V-R --- R-I R-I color mag u_R-I uncertainty flag on R-I --- Nobs Number of observations --- plx Photometric parallax arcsec notes Notes (see notes file) --- Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_1962.xml Chromospherically active stars. X. Spectroscopy and photometry of HD 212280 J/AJ/105/2265 J/AJ/105/2265 Chromospherically active stars. X. Spectroscopy and Chromospherically active stars. X. Spectroscopy and photometry of HD 212280 F C Fekel J C Browning G W Henry M D Morton D S Hall Astron. J. 105 2265 1993 1993AJ....105.2265F Binaries, spectroscopic Radial velocities The system HD 212280 is a chromospherically active double lined spectroscopic binary with an orbital period of 45.284 days and an eccentricity of 0.50. The spectrum is composite with spectral types of G8 IV and F5-8 V for the components. An estimated inclination of 78 deg +/- 8 deg results in masses of 1.7 and 1.4 solar masses for the G subgiant and mid-F star, respectively. The distance to the system is estimated to be 112 pc. Photometric observations obtained between 1987 November and 1992 June reveal that HD 212280 is a newly identified variable star with a V amplitude of about 0.15 mag and a mean period of 29.46 days. Radial velocities are given for each component as are residuals from the derived orbit.
Velocity observations of HD 212280 HJD Heliocentric Julian Date of mid observation d note 'a' -- DDO observation 'b' -- Blended velocity, weight = 0.5 'c' -- central wavelength = 6700 A --- Phase Phase of the observation with zero phase being periastron passage --- Va Observed velocity of component A km/s (O-C)a Residual to the fit or observed minus calculated velocity of A km/s Vb Observed velocity of component B km/s (O-C)b Residual to the fit or observed minus calculated velocity of B km/s Standard Name of the velocity standard star used to determine the observed velocity of HD 212280. --- Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_2265.xml Stellar kinematic groups. I. The Ursa Major Group J/AJ/105/226 J/AJ/105/226 Stellar kinematic groups. I. Ursa Major Group Stellar kinematic groups. I. The Ursa Major Group D R Soderblom M Mayor Astron. J. 105 226 1993 1993AJ....105..226S Associations, stellar Astrometric data Radial velocities Spectroscopy The Ursa Major Group (UMaG) is studied as a test case for the authenticity of Stellar Kinematic Groups, using Coravel radial velocities, recent compilations of astrometric data and new spectroscopic observations. Spectroscopic age indicators, particularly indices of the strength of chromospheric emission, are applied to solar-type candidate members of UMaG, and it is shown that stars that meet the spectroscopic criteria also have kinematics that agree better with the space motions of the nucleus of UMaG than does the starting sample as a whole. The primary limitation on the precision of kinematics is now parallaxes instead of radial velocities. These more restrictive kinematic criteria are then applied to other UMaG candidates and a list summarizing membership is presented.
Stellar kinematic groups Name Group name --- U U space velocity km/s V V space velocity km/s W W space velocity km/s Ref References --- Echelle spectroscopy of UMaG candidates HD Henry Draper number --- m_HD Multiplicity index on HD number --- l_vsini limit flag on vsini --- vsini Rotational velocity km/s l_WHalpha Limit flag on Walpha --- WHalpha Equivalent width of Halpha line 0.1pm l_W8498 Limit flag on W8498 --- W8498 Equivalent width of 8498A feature 0.1pm l_W8542 Limit flag on W8542 --- W8542 Equivalent width of 8542A feature 0.1pm l_W8662 Limit flag on W8662 --- W8662 Equivalent width of 8662A feature 0.1pm l_RHalpha Limit flag on RHalpha --- log(RHalpha) Chromospheric flux ratio (stellar surface flux divided by bolometric flux) for Halpha --- u_RHalpha Uncertainty flag (only for star HD 141003B) --- l_R8498 Limit flag on R8498 --- log(R8498) Chromospheric flux ratio for 8498A feature --- l_R8542 Limit flag on R8542 --- log(R8542) Chromospheric flux ratio for 8542A feature --- l_R8662 Limit flag on R8662 --- log(R8662) Chromospheric flux ratio for 8662A feature --- Spectroscopic membership indicators for UMaG solar-type stars Member a: Probable spectroscopic member b: Possible spectroscopic member c: Probable spectroscopic non-member --- Wooley Number in catalog of Woolley, et al. (1970) --- HD/HDE Henry Draper number --- m_HD/HDE Multiplicity index on HD or HDE number --- HR Harvard Revised (Bright Star) number --- m_HR Multiplicity index on HR number --- Name Other name --- Sp Spectral type number=1 Spectral type from the Bright Star Catalog (Hoffleit & Jaschek 1982), Levato & Abt (1978), Hoffleit et al. (1983), and Woolley, et al. (1970) except for HD 26913/23 (see notes in printed paper). --- B-V (B-V) color from Nicolet (1978) or Woolley et al. (1970) mag u_B-V uncertainty flag on B-V --- Teff Effective temperature K u_Teff uncertainty flag on Teff --- l_R' limit flag on R'(HK). An 'H' indicating that Log(R') is instead an eye estimate of H and K emission strength from Wilson & Woolley (1970) --- logR' Chromospheric flux ratio of the Ca II H and K emission features --- u_logR' uncertainty flag on R' --- n_R(hk) An 'I', indicating logR(hk) is an I(Mg II) value --- logR(hk) Rescaled index, the Mg II h and k emission flux divided by the stellar bolometric flux and reduced to the scale of the Ca II H and K emission in logR' --- l_R(TR) limit flag on R(TR) --- logR(TR) Rescaled index, the emission flux of three strong features in IUE spectra (N I 1240 A, Si IV 1400 A, and C IV 1550 A) combined to produce an index of emission from the star's transition region (TR), reduced to the scale of the Ca II H and K lines as above. --- l_R(Halpha) uncertainty flag on R(Halpha) --- logR(Halpha) Rescaled index, logR(Halpha). --- u_R(Halpha) rms uncertainty on R(Halpha) --- l_R(IRT) uncertainty flag on R(IRT) --- logR(IRT) Rescaled index, for the Ca II infrared triplet. --- l_vsini limit flag on vsini --- vsini Rotational velocity km/s e_vsini rms uncertainty in v sin i km/s Kinematics of UMaG solar-type candidates Kinematics of additional UMaG candidates HD Henry Draper number --- m_HD Multiplicity index on HD number --- plx Parallax from the latest Yale Parallax Catalog (van Altena et al. 1992) mas e_plx rms uncertainty on plx mas pmRA Proper motion in right ascension from the Catalog of Positions and Proper Motions (PPM, Roeser & Bastian 1989) mas/yr e_pmRA rms uncertainty on pmRA mas/yr pmDE Proper motion in declination from the PPM mas/yr e_PMDE rms uncertainty on pmDE mas/yr RV Radial velocity from Evans (1980) km/s e_RV rms uncertainty on RV km/s U Resultant U component of space motion km/s e_U rms uncertainty on U km/s V Resultant V component of space motion km/s e_V rms uncertainty on V km/s W Resultant W component of space motion km/s e_W rms uncertainty on W km/s plx2 Parallax the star must have if V is forced to a value of +2.0 km/s, given its observed radial velocity RV (table7 only) mas MV2 Absolute visual magnitude that follows from the parallax plx2 (table7 only) mag RV2 Radial velocity that results if the parallax is held fixed and the space motion V is forced to +2.0 km/s (table7 only) km/s U2 U space velocity derived from using the observed radial velocity RV2 and the parallax plx2 (table7 only) km/s W2 W space velocity derived from using the observed radial velocity RV2 and the parallax plx2 (table7 only) km/s Summary of UMaG membership Member = Probable Members, ? = Possible Members number=1 +: Probable Members: These are stars for which every indicator supports UMaG membership, which includes: (1) The stars of the nucleus. (2) The probable spectroscopic member stars of Table 5, with Xi Boo excluded. (3) Other stars, such as Sirius, that have well-defined space motions that agree (to within one standard deviation) with the mean motion of the nucleus. ?: Possible Members: In these cases the 3-sigma error ellipsoid overlaps the mean motion of the nucleus. The possible spectroscopic member stars of Table5 that have kinematics in accord with the nucleus are included here. Probable Nonmembers: Any star not listed in Table 11 has been rejected as a UMaG member. --- HD Henry Draper number --- m_HD Multiplicity index on HD number --- HR Harvard Revised number --- m_HR Multiplicity index on HR number --- Name Other name --- Sp Spectral type --- B-V (B-V) color mag Teff Effective temperature K Mv Absolute visual magnitude mag Rem Remarks --- Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_226.xml The eclipsing binary EG Serpentis J/AJ/105/2291 J/AJ/105/2291 The eclipsing binary EG Serpentis The eclipsing binary EG Serpentis J -L Trudel J D Fernie S Mochnacki Astron. J. 105 2291 1993 1993AJ....105.2291T Binaries, eclipsing Photometry, uvby Stromgren b,y photometry of the detached A-type eclipsing binary EG Serpentis was obtained.
Observations JD Heliocentric Julian date (time of observation) d Phase Phase --- y Stromgren y magnitude mag b-y b-y magnitude difference mag b Stromgren b magnitude mag o_by Number of discrete observations which were averaged to give a data point. When o_by = 99.0, the exact number of observations is unknown. --- table1.tex TeX version of table1 Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_2291.xml The evolution of the lithium abundances of solar-type stars. II. The Ursa Major group J/AJ/105/2299 J/AJ/105/2299 Li abundance of solar-type stars. II. The evolution of the lithium abundances of solar-type stars. II. The Ursa Major group D R Soderblom C A Pilachowski S B Fedele B F Jones Astron. J. 105 2299 1993 1993AJ....105.2299S Abundances Associations We draw upon a recent study of the membership of the Ursa Major Group (UMaG) to examine lithium among 0.3 Gyr old solar-type stars. For most G and K dwarfs, Li confirms the conclusions about membership in UMaG reached on the basis of kinematics and chromospheric activity.
Lithium abundances of UMaG solar-type stars Member Membership probability as: a: Probable member b: Possible member c: Probable non-member --- HD Henry Draper number --- m_HD Multiplicity index on HD number --- HR Harvard Revised (Brigth Star) number --- m_HR Multiplicity index on HR number --- Name Other name --- Sp Spectral type --- B-V (B-V) color mag u_B-V Uncertainty flag on B-V --- Teff Effective temperature (average of the temperatures listed in table2) K u_Teff Uncertainty flag on B-V --- l_W(Li)L limit flag on W(Li)L --- W(Li)L Measured equivalent width for Li 6708 A feature from Lick Hamilton spectrograph 0.1pm u_W(Li)L uncertainty flag on W(Li)L --- l_W(Li)K limit flag on W(Li)K --- W(Li)K Measured equivalent width for Li 6708 A feature from Kitt Peak 0.1pm u_W(Li)K uncertainty flag on W(Li)K --- l_W(Li)B limit flag on W(Li)B --- W(Li)B Measured equivalent width for Li 6708 A feature from Boesgaard et al. (1988) 0.1pm W(Li)R Measured equivalent width for Li 6708 A feature from Lick Reticon 0.1pm l_W(Li)E limit flag on W(Li)E --- W(Li)E Measured equivalent width for Li 6708 A feature from ESO 0.1pm l_W(Li)I limit flag on W(Li)I --- W(Li)I Equivalent width for Li 6708 A feature (origin not precised) 0.1pm l_<W(Li)> limit flag on <W(Li)> --- <W(Li)> Adopted mean equivalent width 0.1pm l_log(N(Li)) limit flag on log(N(Li)) --- log(N(Li)) Log of the lithium abundance, log(N(Li)), where log N(H) = 12 --- u_log(N(Li)) Uncertainty flag on B-V --- *Colors and temperatures of UMaG candidates HD Henry Draper number --- m_HD Multiplicity index on HD number --- B-V (B-V) color mag Teff(B-V) Effective temperature inferred from (B-V) K b-y Stromgren color index (b-y) mag Teff(b-y) Effective temperature inferred from color index (b-y) K Beta Stromgren beta index mag Teff(Beta) Effective temperature inferred from beta index K V-I Johnson color index (V-I) mag Teff(V-I) Effective temperature inferred from color index (V-I) K Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_2299.xml Intracluster dust polarization in the Carina nebula J/AJ/105/258 J/AJ/105/258 Intracluster dust polarization in Carina nebula Intracluster dust polarization in the Carina nebula H G Marracho E I Vega F J Vrba Astron. J. 105 258 1993 1993AJ....105..258M Extinction Nebulae Photometry, UBVRI Polarization This catalog presents new UBVRI polarimetric observations of 25 stars and BV polarimetric observations of 60 stars which are embedded in the Carina Nebula. Using these data and photometric data from the literature we have modeled and subtracted the foreground dust contribution in the color excess E(B-V) and the visual polarization.
BV polarimetric observations Note "*" if this is a "front-side" star (22 stars determined to be cluster members and which appear to be least affected by reddening) --- HD Henry Draper number (one star is identified as "RT Car", instead) --- LS Luminous Star (LS) number (Stephenson & Sanduleak 1971). --- Ident Identification (see note 1) --- P(V) Percentage of polarization in V % e_P(V) rms uncertainty on P(V) % Theta(V) Equatorial position angle in V deg e_Theta(V) rms uncertainty on Theta(V) deg P(B) Percentage of polarization in B % e_P(B) rms uncertainty on P(B) % Theta(B) Equatorial position angle in B deg e_Theta(B) rms uncertainty on Theta(B) deg UBVRI polarimetric observations UBVRI intracluster polarization Note "*" if this is a "front-side" star (22 stars determined to be cluster members and and which appear to be least affected by reddening) --- HD Henry Draper number (one star is identified as "RT Car", instead) --- LS Luminous Star (LS) number (Stephenson & Sanduleak 1971). --- Ident Identification (see note 1) --- P374 Percentage of polarization in lambda=0.374 um % e_P374 rms uncertainty on P374 % Theta374 Equatorial position angle in lambda=0.374 um deg e_Theta374 rms uncertainty on Theta374 deg P443 Percentage of polarization in lambda=443 um % e_P443 rms uncertainty on P443 % Theta443 Equatorial position angle in lambda=443 um deg e_Theta443 rms uncertainty on Theta443 deg P563 Percentage of polarization in lambda=0.563 um % e_P563 rms uncertainty on P563 % Theta563 Equatorial position angle in lambda=0.563 um deg e_Theta563 rms uncertainty on Theta563 deg P670 Percentage of polarization in lambda=0.670 um % e_P670 rms uncertainty on P670 % Theta670 Equatorial position angle in lambda=0.670 um deg e_Theta670 rms uncertainty on Theta670 deg P792 Percentage of polarization in lambda=0.792 um % e_P792 rms uncertainty on P792 % Theta792 Equatorial position angle in lambda=0.792 um deg e_Theta792 rms uncertainty on Theta792 deg Observed, foreground, and intracluster color excesses and visual polarizations HD Henry Draper number (one star is identified as "RT Car", instead) --- LS Luminous Star (LS) number (Stephenson & Sanduleak 1971). --- Ident Identification (see note 1) --- E(B-V)O Observed B-V color excess mag E(B-V)F Foreground B-V color excess mag E(B-V)I Intracluster B-V color excess mag P(V)O Observed polarization in V % e_P(V)O rms uncertainty on P(V) % Theta(V)O Observed equatorial position angle in V deg e_Theta(V)O rms uncertainty on Theta(V) deg P(V)F Foreground polarization in V % Theta(V)F Foreground equatorial position angle in V deg P(V)I Intracluster polarization in V % e_P(V)I rms uncertainty on P(V) % Theta(V)I Intracluster equatorial position angle in V deg e_Theta(V)I rms uncertainty on Theta(V) deg UBVRI polarization results HD Henry Draper number (one star is identified as "RT Car", instead) --- LS Luminous Star (LS) number (Stephenson & Sanduleak 1971). --- Ident Identification (see note 1) --- <e_Theta>O Observed dispersion of position angle normalized by the average of the position angle errors --- <e_Theta>I Intracluster dispersion of position angle normalized by the average of the position angle errors --- u_<e_Theta>I A colon, ':', flags two stars that have computed intracluster P(max) < 0.5%, and, hence, small intracluster polarizations in relation to the external errors. The authors have chosen not to extract results from these stars. --- LambdaO Observed wavelength of maximum polarization um e_LambdaO rms uncertainty on LambdaO um PmaxO Observed polarization % e_PmaxO rms uncertainty on PmaxO % Sigma1O Observed unit weight error of least-squares fit % LambdaI Intracluster wavelength of maximum polarization um e_LambdaI rms uncertainty on LambdaI um PmaxI Intracluster polarization % u_PmaxI Uncertainty flag on PmaxI --- e_PmaxI rms uncertainty on PmaxI % Sigma1I Intracluster unit weight error of least-squares fit % tables.tex TeX version of the tables Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_258.xml The Montreal Blue Galaxy Survey. I. First list of ultraviolet-bright candidates J/AJ/105/35 J/AJ/105/35 The Montreal Blue Galaxy Survey. I. First list of The Montreal Blue Galaxy Survey. I. First list of ultraviolet-bright candidates R Cozoil S Demers M Pena S Torres-Peimbert G Fontaine F Wesemael R Lamontagne Astron. J. 105 35 1993 1993AJ....105...35C Galaxies The first results are presented of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of the survey shows that the bulk of the UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey.
First list of UV-bright galaxies MBG Montreal Blue Galaxy (MBG) name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec B Calibrated APM B magnitude mag U-B Calibrated APM U-B color mag IRAS Listed in IRAS catalogues? ("yes" or "no ") --- MB Absolute B magnitude, obtained from B and radial velocity mag CI Cross identification from NASA Extragalactic Database (NED) --- note n = note (see note), s = spectroscopy available --- Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_35.xml A Small Drift Scan Survey for Galaxies in the Northern Sky J/AJ/105/393 J/AJ/105/393 Small Drift Scan Survey Galaxies Northern Sky A Small Drift Scan Survey for Galaxies in the Northern Sky S M Kent M Ramella M Nonino Astron. J. 105 393 1993 1993AJ....105..393K Galaxy catalogs Magnitudes Selected areas The file is an ASCII text file containing data for 1053 galaxies brighter than 18.0 mag. in the filter used. The effective wavelength of this filter for objects that have the color of galaxies closely matches that of Thuan and Gunn r filter. The strip covered in the survey is 12 arcmin wide by 60 degree long. The observations were carried out on the night of 23 May 1990, using the drift scanning technique, with the 24 inch telescope of the Whipple Observatory. The effective integration time was 57 s.
One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected. Important Notice: The published coordinates have errors (up to 6" in the worst case): this is due to a charge smearing problem, which correlates with magnitude. The coordinates in this version are the corrected ones.
*The galaxy catalog ID Number as in the published version the galaxy number 357 is missing in the electronic table: galaxies 357 and 358 seem identical in the printed table. --- RAh 1950 Right Ascension h RAm 1950 Right Ascension minutes min RAs 1950 Right Ascension seconds s DEd 1950 Declination degrees deg DEm 1950 Declination minutes of arc arcmin DEs 1950 Declination seconds of arc arcsec Mag Magnitude mag u_Mag Uncertainty Flag on Magnitude --- Ap Aperture radius used to compute Mag arcsec N. Paul. M. Kuin NSSDC/ADC M. Nonino Trieste 1996 Dec 05 This work has been supported by NSF Grant No. AST 8451724, Nato Grant No. CRG 901016, and a donation from the Digital Equipment Corporation UNKNOWN UNKNOWN * July 1994: the first version was prepared by N. Paul. M. Kuin [NSSDC/ADC] and M. Nonino [Trieste]. * December 1996: the ID number was added at CDS (P. Dubois) J_AJ_105_393.xml IRAS observations of H-alpha selected emission-line galaxies. J/AJ/105/427 J/AJ/105/427 IRAS fluxes of UCM galaxies IRAS observations of H-alpha selected emission-line galaxies. M Rego M Cordero-Gracia J Zamorano J Gallego Astron. J. 105 427 1993 1993AJ....105..427R J/A+AS/118/7 : Photometry + morphology of UCM galaxies (Vitores+, 1996) J/A+AS/120/323 : Long-slit spectroscopy of UCM galaxies (Gallego+ 1996) J/ApJS/95/387 : Universidad Complutense de Madrid list 1 (Zamorano+ 1994) J/ApJS/105/343 : Universidad Complutense de Madrid list 2 (Zamorano+ 1996) Galaxy catalogs Infrared sources We present the results of IRAS observations of the UCM (Universidad Complutense de Madrid) sample of emission-line galaxies, which have been selected from wide-dispersion H{alpha} objective-prism plates. These data are intended to provide a convenient summary of the relevant far-infrared (FIR) properties of these galaxies. Color-color diagrams, as interpreted by theoretical models, suggest that emission from UCM galaxies is mainly due to dust heated directly by photons emitted in active star-forming regions. Statistical analysis of some samples, including the IRAS minisurvey and blue selected objective-prism samples, have been performed. Comparisons, based on FIR luminosity distributions, with the IRAS minisurvey make evident the lower metallicity of the UCM galaxies which cannot be considered as a parent population of IRAS-detected galaxies. The FIR luminosity distributions of different samples have been compared using nonparametric methods and the best correlation has been found for the UCM and Wasilewski samples. Finally, a more detailed analysis of a UCM subsample has been performed from a three component model in order to get information concerning the fractional contribution of disk, star formation activity, and nonthermal mechanisms operating in the UCM galaxies.
IRAS
UCM galaxy sample UCM UCM designation --- l_F12um Limit flag on F12um --- F12um Flux density at 12{mu}m Jy l_F25um Limit flag on F25um --- F25um Flux density at 25{mu}m Jy l_F60um Limit flag on F60um --- F60um Flux density at 60{mu}m Jy l_F100um Limit flag on F100um --- F100um Flux density at 100{mu}m Jy mpg Photographic magnitude mag z Redshift --- Names Other names number=1 CG: Pesch et al., 1991ApJS...76.1043P HOLM: Holmberg, 1937AnLun...6....1H KARA: Karachentsev, 1972, Cat. <VII/77> KAZ: Kazarian & Kazarian, 1980Afz....16...17K KUG: KISO (Takase & Hiyauchi-Isobe, 1991, See Cat. <VII/179>) M: Vorontsov-Velyaminov & Krasnogorskaja, 1962, Cat. <VII/62> MK: Markarian & Lipovetskii, 1971-79, See Cat. <VII/172> N: NGC, Dreyer, 1888, See Cat. <VII/118> PG: Palomar Green (Green et al., 1986, Cat. <II/207>) REIZ: Reiz, 1941AnLun...9....1R U: UGC Nilson, 1973, Cat. <VII/26> UM: University of Michigan Survey (MacAlpine & Williams, 1981, Cat. <VII/171>) WAS: Wasilewski, 1983ApJ...272...68W ZWG: Zwicky & Herzog, 1963, Cat. <VII/4> --- Contributions of the three components to the UCM observed FIR fluxes. UCM UCM designation --- d Contribution fraction of normal disk (d) component % b Contribution fraction of starburst (b) component % s Contribution fraction of Seyfert (s) component % sigma Computed error % James Marcout, Patricia Bauer CDS 1998 Oct 20 UNKNOWN UNKNOWN Prepared via OCR at CDS, and proof-read by Heinz Andernach (heinz@astro.ugto.mx). J_AJ_105_427.xml OB Associations and Spiral Structure in the Southern Arm of M33 J/AJ/105/499 J/AJ/105/499 OB Associations and Sprial Structure in M33 OB Associations and Spiral Structure in the Southern Arm of M33 M W Regan C D Wilson Astron. J. 105 499 1993 1993AJ....105..499R Galaxies, nearby Photometry, UBV This file contains UBV photometry for the brightest stars in the southern spiral arm of M33. All stars brighter than V=21 are included in this file. For details on the observations and data reduction see reference. All the data is in ASCII format of the file.
The observations ID Star ID --- RAh Right Ascension (1950) h RAm Right Ascension (1950) min RAs Right Ascension (1950) s X X Coordinate pix V V band Magnitude mag B B band Magnitude mag U U band Magnitude (blank if undetermined) mag B-V B-V Magnitude mag U-B U-B Magnitude (blank if undetermined) mag ass Association number containing star --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Y Y Coordinate pix uV V uncertainty mag uB B uncertainty mag uU U uncertainty (blank if undetermined) mag M. W. Regan and N. G. Roman NASA/NSSDC/ADC 1994 Sep 19 J_AJ_105_499.xml The Large Magellanic Cloud cluster NGC 1835: photometry of the RR Lyrae stars J/AJ/105/527 J/AJ/105/527 The Large Magellanic Cloud cluster NGC 1835: The Large Magellanic Cloud cluster NGC 1835: photometry of the RR Lyrae stars A R Walker Astron. J. 105 527 1993 1993AJ....105..527W Photometry, BV Stars, variable Photometry is presented for the RR Lyrae variables in the Large Magellanic Cloud (LMC) cluster NGC 1835. Sixteen new variables have been discovered. Due to the extreme crowding of the LMC field stars, the scatter of the light curves and mean magnitudes is greater than that found for other LMC clusters studied under similar conditions. The derived parameters of the light curves yield E(B-V) = 0.13 and [Fe/H] = -1.8, consistent with previous measurements. The complete sample of RR Lyraes has mean magnitudes <V> = 19.38, <B> = 19.70. If a distance modulus of 18.5 mag for the LMC is assumed, then in the mean the NGC 1835 RR Lyraes have <Mv> = 0.48, almost identical to the average found by the same procedure for the six other LMC clusters.
RR Lyr var. photometry HJD Heliocentric Julian Date number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper d GR/V1V GR/V1 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V1B GR/V1 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V3V GR/V3 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V3B GR/V3 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V4V GR/V4 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V4B GR/V4 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V5V GR/V5 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V5B GR/V5 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V6V GR/V6 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V6B GR/V6 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V7V GR/V7 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V7B GR/V7 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V8V GR/V8 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V8B GR/V8 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V9V GR/V9 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V9B GR/V9 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V11V GR/V11 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V11B GR/V11 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V13V GR/V13 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V13B GR/V13 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V14V GR/V14 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V14B GR/V14 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V15V GR/V15 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V15B GR/V15 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V16V GR/V16 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V16B GR/V16 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V17V GR/V17 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V17B GR/V17 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V18V GR/V18 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V18B GR/V18 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V19V GR/V19 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V19B GR/V19 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V20V GR/V20 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V20B GR/V20 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V22V GR/V22 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V22B GR/V22 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V23V GR/V23 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V23B GR/V23 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V24V GR/V24 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V24B GR/V24 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V25V GR/V25 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V25B GR/V25 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V26V GR/V26 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V26B GR/V26 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V27V GR/V27 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V27B GR/V27 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V28V GR/V28 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V28B GR/V28 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V29V GR/V29 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V29B GR/V29 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V30V GR/V30 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V30B GR/V30 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V31V GR/V31 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V31B GR/V31 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V32V GR/V32 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V32B GR/V32 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V33V GR/V33 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V33B GR/V33 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V34V GR/V34 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V34B GR/V34 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V35V GR/V35 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V35B GR/V35 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V36V GR/V36 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V36B GR/V36 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V37V GR/V37 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V37B GR/V37 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V38V GR/V38 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V38B GR/V38 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V39V GR/V39 V magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag GR/V39B GR/V39 B magnitude number= GR/V1 to GR/V23: stars discovered by Graham J.A. & Ruiz M.T. (1974, AJ, 79, 363, GR) GR/V24 to GR/v39: new variable stars from this paper mag Derived quantities for the var. stars GR/V GR/V denomination --- Walker Walker denomination --- P(GR) GR period d P(W) Walker period d <V> Mean V magnitude mag u_<V> uncertainty flag on <V> --- <B> Mean B magnitude mag u_<B> uncertainty flag on <B> --- B-V B-V color mag u_B-V uncertainty flag on B-V --- (B-V)min Minimun B-V color mag u_(B-V)min uncertainty flag on (B-V)min --- Av Absorption in V mag u_Av uncertainty flag on Av --- Ab Absorption in B mag u_Ab uncertainty flag on Ab --- Note See note number=1 1: GR1. Periods of several days are poorly constrained by the data available, and other periods with a frequency spacing of ~0.03 day^-1^ are possible, although giving noticeably poorer light-curves. With the adopted period the phases near maximum have been missed, even so, the star is much too faint to be an LMC Cepheid which would be expected to have <V> = 15.4 2: GR2. Red variable. Mean magnitudes: HJD=2448207 (V=16.19, B=18.16), HJD=2448248 (V=16.89, B=18.91), HJD=2448279 (V=17.53, B=19.40) 3: GR4. Eclipsing binary 4: GR9. Low amplitude, noisy light-curve. The period is uncertain. A star of similar magnitude is at 1.5 arcsec separation. 5: GR10. Not measured 6: GR11. The GR period was adopted. The mean magnitudes are very faint, probably due to elevation of the sky by an adjacent bright star. 7: GR12. This star is the closest known variable to the cluster center. Only a few measurements were possible, and these scatter badly when passed with the GR period, so have been discussed. 8: GR16. Only a few useful observations, with a large phase gap. 9: GR17. Large phase gap due to the period being almost exactly 0.5 days. 10: GR20. GR period adopted. 11: GR21. No such star is marked on the GR chart although a period and light curve are given. None of the new variables found match the period. 12: GR37. Blended with another star. Photometry is very bright, almost certainly due to insufficient subtraction of the companion star. --- Patricia Bauer CDS 1994 Jul 06 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_527.xml A study of the rich cluster of galaxies A119. J/AJ/105/788 J/AJ/105/788 Study of Abell 119 A study of the rich cluster of galaxies A119. D Fabricant M Kurtz M Geller A Zabludoff P Mack G Wegner Astron. J. 105 788 1993 1993AJ....105..788F Clusters, galaxy Redshifts We report 60 new radial velocities, as well as new photographic and CCD photometry.
Photometric & Spectroscopic data Origin Origin of the data: PDS or CCD --- Dressler Dressler <VII/174> Designation --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec Rmag Magnitude in R-band mag cz Velocity km/s e_cz Mean error on cz km/s MType Morphological type --- r_cz Reference of velocity number=1 the codes for references are: MQ = Melnick & Quintana (1981AJ.....86.1567M) RC3 = de Vaucouleurs et al., 1991 (Cat. <VII/155>) HDTL = Huchra et al. (1983ApJS...52...89H) S = Sandage (1978AJ.....83..904S) KH = Kinman & Hintzen (1981PASP...93..405K) blank: from this study --- James Marcout, Francois Ochsenbein CDS 1997 Apr 01 UNKNOWN UNKNOWN * April 1994: Keypunched at CDS * April 1997: Error corrected in galaxy at 00 54 31.5 -01 11 22 thanks to William Burgett <burgett@lesol1.dseg.ti.com> J_AJ_105_788.xml Energy distributions of radio galaxies J/AJ/105/853 J/AJ/105/853 Energy distributions of radio galaxies Energy distributions of radio galaxies C Impey L Gregorini Astron. J. 105 853 1993 1993AJ....105..853I Galaxies, radio Photometry, infrared Far-infrared observations of 140 radio galaxies from the 3CR and B2 catalogs are presented. The galaxies span a range of over four order of magnitude in the radio power, from weak nuclear sources in nearby galaxies, to powerful FR II doubled-lobed sources at moderate redshift. Scanned or pointed observations with IRAS detect 38 of the radio galaxies in at least one waveband; 21 are detected at both 60 and 100 {mu}m.
B2 and 3CR radio galaxies Name Galaxy name --- z Redshift --- mv Visual magnitude mag S408 Total radio flux at 408MHz mJy l_S5 Limit flag on S5 --- S5 Core radio flux at 5GHz mJy l_S12 Limit flag on S12 --- S12 IRAS flux density at 12 microns mJy e_S12 rms uncertainty on S12 mJy l_S25 Limit flag on S25 --- S25 IRAS flux density at 25 microns mJy e_S25 rms uncertainty on S25 mJy l_S60 Limit flag on S60 --- S60 IRAS flux density at 60 microns mJy e_S60 rms uncertainty on S60 mJy l_S100 Limit flag on S100 --- S100 IRAS flux density at 100 microns mJy e_S100 rms uncertainty on S100 mJy Patricia Bauer CDS 1994 Jul 05 Chris Impey <impey@as.arizona.edu> J_AJ_105_853.xml Star formation in dwarf irregular galaxies: DDO 210 and NGC 3109 J/AJ/105/894 J/AJ/105/894 Star formation in dwarf irregular galaxies: Star formation in dwarf irregular galaxies: DDO 210 and NGC 3109 L Greggio G Marconi M Tosi P Focardi Astron. J. 105 894 1993 1993AJ....105..894G Galaxies Photometry, BV Deep CCD photometry has been obtained of two regions in DDO 210 and three regions in NGC 3109, reaching V = 24 with the required accuracy of Sigma(V) <= 0.1 mag.
Principal parameters from the selected stars in DDO 210 region A Principal parameters from the selected stars in DDO 210 region B N Star number --- X X pixel coordinate, referred to the bottom left corner of each frame pix Y Y pixel coordinate pix V V magnitude mag B-V B-V color mag Principal parameters from the selected stars in NGC 3109 region A Principal parameters from the selected stars in NGC 3109 region B Principal parameters from the selected stars in NGC 3109 region C N Star number --- X X pixel coordinate, referred to the bottom left corner of each frame pix Y Y pixel coordinate pix V V magnitude mag B-V B-V color mag V-R V-R color mag Patricia Bauer CDS 1994 Jun 20 AAS CD-ROM series, Volume 1, 1993 J_AJ_105_894.xml Dynamics of the young binary LMC cluster NGC 1850 J/AJ/105/938 J/AJ/105/938 Dynamics of the young binary LMC cluster NGC 1850 Dynamics of the young binary LMC cluster NGC 1850 P Fischer D L Welch M Mateo Astron. J. 105 938 1993 1993AJ....105..938F Clusters, open Photometry, BV In this paper we examine the age and internal dynamics of the young binary LMC cluster NGC 1850 using BV CCD images and echelle spectra of 52 supergiants.
BV photometry ID Running number --- X X position on the CCD --- Y Y position on the CCD --- V V-band magnitude mag B-V B-V color mag Patricia Bauer CDS 1994 Jul 05 Philippe Fischer <philf@physics.att.com> J_AJ_105_938.xml Massive stars near Eta Carinae: the stellar content of Tr 14 and Tr 16. J/AJ/105/980 J/AJ/105/980 Massive stars near Eta Carinae: the stellar content Massive stars near Eta Carinae: the stellar content of Tr 14 and Tr 16. P Massey J Johnson Astron. J. 105 980 1993 1993AJ....105..980M Clusters, globular Photometry, UBV Spectral types The stellar content of the region around {eta} Car is investigated using CCD photometry and spectroscopy.
Photometry and cross-identifications (tables 1 and 2) Star Star designation --- X Position (positive toward West) pix Y Position (positive toward North) pix V derived from CCD photometry mag u_V Uncertainty notes on V: "bl" indicates a blended image --- U-B derived from CCD photometry mag u_U-B Uncertainty notes on U-B --- B-V derived from CCD photometry mag u_B-V Uncertainty notes on B-V --- Feinstein Designation in clusters Tr 14 and Tr 16 (A&AS 12, 331, 1973 ; AJ 87, 1012, 1982) --- Other Other designation (HD or CPD) --- The brightest and bluest stars Star Star designation as above --- X Position (positive toward West) pix Y Position (positive toward North) pix RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) - DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec V derived from CCD photometry mag u_V "bl" indicates a blended image --- B-V derived from CCD photometry mag u_B-V --- U-B derived from CCD photometry mag u_U-B --- Q Reddening-free parameter = (U-B)-0.72*(B-V) mag Sp(New) Spectral type from this study --- Sp(W) Spectral type from Walborn (AJ 77, 312, 1972; ApJ 179, 517, 1973; AJ 78, 1067, 1973; AJ 87, 1300, 1982) --- Sp(MGL) Spectral type from Morell, Garcia & Levato, 1988, PASP 100, 1431 --- Comment Designations in clusters Tr 14 (A&AS 12, 331, 1973) or Tr 16 (A&AS 12, 331, 1973 ; AJ 87, 1012, 1982) --- New Spectral types Star Star designation as above --- X Position (positive toward West) pix Y Position (positive toward North) pix V derived from CCD photometry mag u_V "bl" indicates a blended image --- B-V derived from CCD photometry mag u_B-V Uncertainty notes on B-V --- U-B derived from CCD photometry mag u_U-B Uncertainty notes on U-B --- Q Reddening-free parameter = (U-B) - 0.72*(B-V) mag Sp(New) Spectral type from this study --- Comment Designations in cluster Tr 14 or Tr 16 --- Distance & Reddening derived from spectroscopy Star Star designation as above --- E(B-V) Color excess mag E(U-B) Color excess mag Ratio Ratio E(U-B)/E(B-V) --- Sp Spectral type --- Av Absorption derived from spectral type mag V0 Dereddened magnitude derived from spectral type mag Mv Absolute magnitude derived from spectral type mag m-M Distance modulus derived from spectral type mag James Marcout, Francois Ochsenbein CDS 1994 Apr 07 UNKNOWN UNKNOWN Keypunched at CDS. Tables 1 and 2 have been merged into a single file. J_AJ_105_980.xml Luminosity functions for post-turnoff stars in globular clusters. I. NGC 288 J/AJ/106/1024 J/AJ/106/1024 BV photometry in NGC 288 Luminosity functions for post-turnoff stars in globular clusters. I. NGC 288 P A Bergbusch Astron. J. 106 1024 1993 1993AJ....106.1024B Clusters, globular Photometry, BV *** No Description Available ***
The photometry for all stars (see above note) ID Star number in cluster --- X Position (North lies in the direction of decreasing X) pix Y Position (West lies in the direction of decreasing Y) pix Bmag B magnitude mag e_Bmag Standard deviation on B mag Vmag V magnitude mag e_Vmag Standard deviation on V mag chi mean chi value which indicates the quality of the profile fit --- Francois Ochsenbein CDS 1993 Dec 23 Peter A. Bergbush (bergbush@deneb.phys.uregina.ca) UNKNOWN UNKNOWN Notes: The "appendix" file reaches approximately 1.5 magnitudes fainter than the table 7 in Appendix B of the paper, but the fainter data are highly uncertain. The data were derived from profile-fitting photometry as performed by DAOPHOT and the stand alone routine ALLSTAR, both of which have been developed by Peter Stetson of the DAO, Victoria, B.C. J_AJ_106_1024.xml The evolution of the lithium abundances of solar-type stars. III. The Pleiades J/AJ/106/1059 J/AJ/106/1059 Lithium in the Pleiades The evolution of the lithium abundances of solar-type stars. III. The Pleiades D R Soderblom B F Jones S Balachandran J R Stauffer D K Duncan S B Fedele J D Hudon Astron. J. 106 1059 1993 1993AJ....106.1059S Abundances Clusters, open We report new measurements of lithium in more than 100 Pleiades F, G, and K dwarfs. Abundances were determined from spectrum synthesis fits to the data as well as from use of new curves of growth for the Li 6708 A feature.
Observations of Lithium in Pleiades F, G, and K dwarfs fgk fgk number from Soderblom et al. 1993, ApJS, 85, 315 (hereafter SSHJ) --- name Hertzsprung (H II) designation. A "P" prefix denotes a Pels star. --- Sp Spectral type --- (B-V)0 Dereddened (B-V) mag u_(B-V)0 Uncertainty flag on (B-V)0 --- Teff Effective temperature K l_vsini Limit flag on vsini --- vsini Rotational velocity km/s u_vsini uncertainty flag on vsini --- n_vsini 'S' indicating a double-lined spectroscopic binary whose vsini values are given in table2 of SSHJ (SB2). --- log(RHalpha) Ratio of the Halpha flux to the stellar bolometric flux, log R(Halpha) from SSHJ --- log(R8542) Ratio of the 8542 A Ca II line flux to the stellar bolometric flux, logR(8542) from SSHJ --- W7699 Equivalent width of K I 7699A line 0.1pm W6717 Equivalent width of Ca I 6717 A line 0.1pm n_W6717 Note on W6717. See note number=1 A '*' indicates that equivalent width of the line has been compensated for spectrum dilution by the following factors: H II 102, 1.33; H II 173, 1.40; H II 248 and 2147, 1.20; H II 298, 571, 1100, and 2406, 1.10; H II 320, 1.15; H II 1101, 1.25. --- l_W6708 Limit flag on W6708 --- W6708 Equivalent width of Li I 6708 A line, corrected for Fe I 6707.441. 0.1pm u_W6708 Uncertainty flag on W6708 --- n_W6708 Note on W6708. See note number=1 A '*' indicates that equivalent width of the line has been compensated for spectrum dilution by the following factors: H II 102, 1.33; H II 173, 1.40; H II 248 and 2147, 1.20; H II 298, 571, 1100, and 2406, 1.10; H II 320, 1.15; H II 1101, 1.25. --- q Source and quality code number=2 Source and quality code: Bo = Boesgaard et al. 1988b, ApJ, 327, 389 Bu = Butler et al. 1987, ApJ, 319, L19 P = Pilachowski et al. 1987, PASP, 99, 1288 Codes a to d denote Lick data and are in descending order of quality, with approximate uncertainties of 12, 18, 25, and 40 mA, respectively --- l_log(N(Li)) Limiting character for lithium abundance --- log(N(Li)) Abundance of lithium (scale logN(H)=12) --- u_log(N(Li)) Uncertainty flag on log(N(Li)) --- *Lithium abundances for the 6708 A feature *Lithium abundances for the 6104 A feature log(W6708) Equivalent width of Li 6708 line 0.1pm logN(Li)1 Li abundance for Teff = 4000 K --- logN(Li)2 Li abundance for Teff = 4250 K --- logN(Li)3 Li abundance for Teff = 4500 K --- logN(Li)4 Li abundance for Teff = 4750 K --- logN(Li)5 Li abundance for Teff = 5000 K --- logN(Li)6 Li abundance for Teff = 5250 K --- logN(Li)7 Li abundance for Teff = 5500 K --- logN(Li)8 Li abundance for Teff = 5750 K --- logN(Li)9 Li abundance for Teff = 6000 K --- logN(Li)10 Li abundance for Teff = 6250 K --- logN(Li)11 Li abundance for Teff = 6500 K --- Patricia Bauer CDS 1994 Sep 12 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_1059.xml The evolution of the lithium abundances of solar-type stars. IV. Praesepe J/AJ/106/1080 J/AJ/106/1080 Lithium in Praesepe The evolution of the lithium abundances of solar-type stars. IV. Praesepe D R Soderblom S B Fedele B F Jones J R Stauffer C F Prosser Astron. J. 106 1080 1993 1993AJ....106.1080S Abundances Clusters, open Echelle observations are presented of lithium in 63 F and G dwarfs of the Praesepe cluster.
Observations of lithium in Praesepe solar-type stars KW Number in catalog of Klein-Wassink (1927) --- VL Number in catalog of Vanderlinden (1933) --- Sp Spectral type, where available, taken from Corbally & Garrison (1986), Corbally & Garrison (1983) or Wilson (1963), in order of preference ---- B-V B-V color from Mendoza (1967) mag V-I Johnson (V-I) from Mendoza (1967) mag Teff Effective temperature K l_WLi Limit flag on WLi --- WLi Equivalent width of Li 6708 0.1nm l_log(N(Li)) Limit flag on N(Li) --- log(N(Li)) Lithium abundance (scale log N(H) = 12) --- Patricia Bauer CDS 1994 Sep 14 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_1080.xml The kinematics of dense clusters of galaxies. I. The data. J/AJ/106/1273 J/AJ/106/1273 The kinematics of dense clusters of galaxies. I. The kinematics of dense clusters of galaxies. I. The data. A I Zabludoff M J Geller J P Huchra M S Vogeley Astron. J. 106 1273 1993 1993AJ....106.1273Z Clusters, galaxy Redshifts Redshifts have been measured in the fields of the 31 R>=1 Abell clusters with 0.02<z<0.05 and |bII|>30. At least ten of the fields are severely contaminated by superimposed velocity peaks. Mean velocities and velocity dispersions have been derived for the 25 dense peaks in the sample.
Cluster data Cluster Abell cluster designation --- Name Galaxy name number=1 Names with RA given with five digits are normally from Zwicky catalogues; the other (with four digits in RA, starting or not with the letter A) are anonymous galaxies. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec B(0) Integrated magnitude mag n_B(0) Origin of B(0) number=2 C = CCD photometry (CfA redshift survey 1992) H = Zwicky magnitude split by observers K = Markarian catalogue of galaxies (1967) M = MCG (Vorontsov-Velyaminov et al. 1962-68) P = observer's eye estimate R = RC1 (de Vaucouleurs & de Vaucouleurs 1964) --- RV Velocity km/s e_RV Mean error on V km/s Francois Ochsenbein CDS 1994 Apr 20 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_106_1273.xml Dynamics of the globular cluster NGC 362 J/AJ/106/1508 J/AJ/106/1508 Dynamics of the globular cluster NGC 362 Dynamics of the globular cluster NGC 362 P Fischer D L Welch M Mateo P Cote Astron. J. 106 1508 1993 1993AJ....106.1508F Clusters, globular Radial velocities Radial velocities have been derived in the globular cluster NGC 362 using a combination of V-band CCD images and echelle spectra of the member red giants.
Radial velocities Name Star name --- RAh Right ascension 2000.0 h RAm Right ascension 2000.0 min RAs Right ascension 2000.0 s DE- Declination sign --- DEd Declination 2000.0 deg DEm Declination 2000.0 arcmin DEs Declination 2000.0 arcsec Radius Derived projected radius arcsec PA Position angle deg HJD Heliocentric Julian Date d VR Observed radial velocity km/s u_VR rms uncertainty on VR km/s <VR> Mean radial velocity for stars with multiple observations km/s e_<VR> rms uncertainty on <VR> km/s Chi2 Chi squared for stars with multiple observations --- n_Chi2 Number of degrees of freedom of Chi2 --- Comment Comments --- Patricia Bauer CDS 1994 Jun 28 Phil Fischer. J_AJ_106_1508.xml New proper motions in the globular cluster M5 J/AJ/106/1524 J/AJ/106/1524 Proper motions in M5 New proper motions in the globular cluster M5 R F Rees Jr. Astron. J. 106 1524 1993 1993AJ....106.1524R Clusters, globular Photometry, BV Proper motions New proper motions have been derived from reductions of PDS microdensitometer scans of 17 Yerkes refractor plates spanning an epoch range of 88 years for 515 stars down to V~15.6 in the region of the globular cluster M5. Photographic photometry in B and V has been obtained for these stars from these scans and scans of six Yerkes reflector plates. The present proper motions have significantly improved precision compared to Cudworth [AJ, 84, 1866 (1979)]. Membership probabilities have been derived from the new proper motions. and radial velocity dispersions.
M5 positions, proper motions, photometry, and membership probabilities. Ident Star identifications number=1 B : Barnard (1931) Lowercase letter (with no number following): Arp (1955a) Roman numeral followed by a dash : Arp (1955b) and Buonanno (1981) Uppercase letter (with no number following): Arp (1962) Roman numeral with no dash : Arp (1962) Z : Zhukov (1971) ZNG : UV-bright star from Zinn et al. (1972) V : Variable star from Sawyer Hogg (1973) C : Cudworth (1979) S : Sanduleak (1989) R : This study -------------------------------------------------------------------------------- References: Arp H.C., 1955a, AJ, 60, 1 Arp H.C., 1955b, AJ, 60, 317 Arp H.C., 1962, ApJ, 135, 311 Barnard E.E. 1931, Publ. Yerkes Obs., Vol. 6 Buonann R. et al. 1981, MNRAS, 196, 435 Cudworth K.M. 1979, AJ, 84, 1866 Sanduleak N. 1989, 1989, ApJS, 71, 713 Sawyer Hogg H. 1973, Publ. David Dunlap Obs., Vol. 3, No. 6 Zhukov L.V. 1971, Trudy Pulkova Obs., Ser. 2, 78, 160 Zinn R.J. et al. 1972, A&A, 18, 390 This study --- X X offset from cluster center and aligned close to R.A. and Dec. (equator & equinox 1950, epoch 1975) arcsec Y Y offset from cluster center arcsec pmX Relative proper motion in X 10-5arcsec/yr e_pmX rms uncertainty on pmX 10-5arcsec/yr pmY Relative proper motion in Y 10-5arcsec/yr e_pmY rms uncertainty on pmY 10-5arcsec/yr Vmag V magnitude mag B-V B-V color mag Member Membership probability % Patricia Bauer CDS 1994 Sep 14 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_1524.xml NGC 2287: an important intermediate-age open cluster J/AJ/106/1533 J/AJ/106/1533 NGC 2287 NGC 2287: an important intermediate-age open cluster G L H Haris P M Fitzgerald S Mehta B C Reed Astron. J. 106 1533 1993 1993AJ....106.1533H Clusters, open Photometry, ubvy, beta Photometry, UBV Spectral types Photoelectric UBV photometry has been obtained for 100 stars, uvbyBeta photometry for 39 stars and MK spectral types for 80 stars in the field of NGC 2287.
UBV photometry in NGC 2287 HFMR Identification number number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- MembA Adopted cluster membership, based on overall indicators number=1 Codes for cluster membership indicators B Probable binary member of cluster. b Possible binary member of cluster. C Possibly C+E. E Probably evolved. G Probable member of background group. g Possible member of background group. F Probable field object. f Possible field object. N Non-member of cluster or background group. n Possible non-member of cluster or background group. M Probable cluster member. m Possible cluster member. u No U-B but photometry consistent with membership at mean cluster extinction X Non-member due to incorrect color excess. Z Probable member on the ZAMS. z Possibly member on the ZAMS. --- MembE Excess membership indicator based on consistency relation to the main sequence number=1 Codes for cluster membership indicators B Probable binary member of cluster. b Possible binary member of cluster. C Possibly C+E. E Probably evolved. G Probable member of background group. g Possible member of background group. F Probable field object. f Possible field object. N Non-member of cluster or background group. n Possible non-member of cluster or background group. M Probable cluster member. m Possible cluster member. u No U-B but photometry consistent with membership at mean cluster extinction X Non-member due to incorrect color excess. Z Probable member on the ZAMS. z Possibly member on the ZAMS. --- MembS Spectrum membership indicator based on agreement of photometric and spectroscopic type number=1 Codes for cluster membership indicators B Probable binary member of cluster. b Possible binary member of cluster. C Possibly C+E. E Probably evolved. G Probable member of background group. g Possible member of background group. F Probable field object. f Possible field object. N Non-member of cluster or background group. n Possible non-member of cluster or background group. M Probable cluster member. m Possible cluster member. u No U-B but photometry consistent with membership at mean cluster extinction X Non-member due to incorrect color excess. Z Probable member on the ZAMS. z Possibly member on the ZAMS. --- MembL Luminosity membership indicator based on agreement of photometric and spectroscopic class number=1 Codes for cluster membership indicators B Probable binary member of cluster. b Possible binary member of cluster. C Possibly C+E. E Probably evolved. G Probable member of background group. g Possible member of background group. F Probable field object. f Possible field object. N Non-member of cluster or background group. n Possible non-member of cluster or background group. M Probable cluster member. m Possible cluster member. u No U-B but photometry consistent with membership at mean cluster extinction X Non-member due to incorrect color excess. Z Probable member on the ZAMS. z Possibly member on the ZAMS. --- MembZ ZAMS+CMD membership indicator based on position in color-magnitude diagram, especially for near-ZAMS (Zero-Age Main-Sequence) stars number=1 Codes for cluster membership indicators B Probable binary member of cluster. b Possible binary member of cluster. C Possibly C+E. E Probably evolved. G Probable member of background group. g Possible member of background group. F Probable field object. f Possible field object. N Non-member of cluster or background group. n Possible non-member of cluster or background group. M Probable cluster member. m Possible cluster member. u No U-B but photometry consistent with membership at mean cluster extinction X Non-member due to incorrect color excess. Z Probable member on the ZAMS. z Possibly member on the ZAMS. --- Name Identification numbers from other authors, Cox (1954), Hoag et al. (1961), or Ianna et al. (1987) number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Vmag Mean V magnitude number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 mag Var Variability flag, 'V', or blank number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- e_Vmag rms uncertainty on V magnitude. number=2 Errors reported in this table are based on observational error and estimates from other authors. For derived quantities the errors are those propagated through the photometric dereddening process. 10-3mag B-V Mean (B-V) color number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 mag e_B-V rms uncertainty on mean (B-V) color number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 10-3mag U-B Mean (U-B) color number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 mag e_U-B rms uncertainty on mean (U-B) color number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 10-3mag Sp Spectral type derived from photometric data number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- u_Sp Uncertainty flag on spectral type number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- LC Luminosity class derived from photometric data number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- u_LC Uncertainty flag on luminosity class number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Nobs1 Number of observations in this paper number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Nobs2 Number of observations in Feinstein et al., (1978) number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Nobs3 Number of observations in Cox (1954) number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Nobs4 Number of observations in Eggen (1974) number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Nobs5 Number of observations in Hoag et al. (1961) (photoelectric) number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Nobs6 Number of observations in Hoag et al. (1961) (photographic) number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Nobs7 Number of observations in Ianna et al. (1987) number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- MKSp Adopted MK class, primarily from this paper. Classes in parentheses, "()", are from other sources. number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- V0 Intrinsic V(0) magnitude derived by WATREDAO number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 mag u_V0 Uncertainty flag on intrinsic V(0) magnitude number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- Var A 'V' indicates variability number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- e_V0 rms uncertainty on V(0). number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 10-3mag u_e_V0 rms uncertainty on e_V(0). number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- (B-V)0 Intrinsic (B-V)(0) color derived by WATREDAO number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 mag u_(B-V)0 Uncertainty flag on (B-V)0 number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- e_(B-V)0 rms uncertainty on (B-V)(0). number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 10-3mag u_e_B-V Uncertainty flag on e_(B-V)0 number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 --- DistMod (V(0)-Mv) derived assuming the star lies on the Zero-Age Main-Sequence number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 mag e_DistMod rms uncertainty on distance modulus number= Cox, A. N. 1954, ApJ, 119, 188 Eggen, O. J. 1974, ApJ, 188, 59 Feinstein, A., Cabrera, A. L. & Claria, J. J. 1978, A&AS, 43, 241 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., & Hallam, K. L., & Sharpless, S. 1961, Pub. U.S. Naval Obs., 17, 349 Ianna, P. A., Adler, D. S., & Faudree, E. F. 1987, AJ, 93, 347 10-3mag Notes Notes number=3 A Near A hump in two color diagram; color excess could be too large. H Near F hump in two color diagram; color excess could be too large or small. 1 Smallest color excess chosen. 2 Second smallest color excess chosen. 3 Possibly contaminated by a nearby object. 4 Duplicity indicated by some MK classifications. 5 MK adopted is not from this study and is shown in brackets. 6 Binary; 0.5 to 0.8 magnitudes and more than 2 sigma above ZAMS. 7 Colors and spectrum incompatible. 8 Photometric spectrum and colors may be uncertain for bright giants. 9 Color excess chosen to suit membership and/or mean color excess. 10 Color excess more than 1 sigma from the mean. 12 Bad U-B? 13 Deconvolved binary star. 15 Luminosity class incompatible with membership. 16 Color excess too high for membership, but star not necessarily excluded. 17 Outside cluster radius suggested by star counts. 18 Luminosity class supports duplicity. 19 6, 11, and 12. 20 7, 10, and 14. 21 Quoted photometry is from Ianna, Adler and Faudree. 22 U-B from Ianna et al. 23 10, 16, 17, and 21. 24 10, 17, and 21. : A colon indicates that the data are of poorer than average quality, so that conclusions in the footnotes which the colon follows are uncertain, suspect... For HFMR 1ABR, 3" is the angular separation for the A and B components. For HFMR 92, 5" is the angular separation for the A and B components. --- uvbyBeta photometry in NGC 2287 HFMR Identification number number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 --- V Mean V magnitude number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 mag e_V rms uncertainty on mean V magnitude number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 10-3mag b-y Mean (b-y) color number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 mag e_b-y rms uncertainty on mean (b-y) color number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 10-3mag m1 Mean m(1) index number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 mag e_m1 rms uncertainty on mean m(1) index number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 10-3mag c1 Mean c(1) index number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 mag e_c1 rms uncertainty on mean c(1) index number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 10-3mag Beta Mean Beta number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 mag e_Beta rms uncertainty on mean Beta number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 10-3mag HF Number of photometric observations from this paper number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 --- E1 Number of photometric observations taken from Eggen (1974) number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 --- E2 Number of photometric observations taken from Eggen (1981) number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 --- Code Code for method used to derive individual values of E(b-y) and V(0)-Mv: A Crawford (1979) A0 Claria (1974) adapted from Stromgren (1966) as described by Eggen (1981) B Crawford (1978) F Crawford (1975) number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 --- E(b-y) Reddening E(b-y) number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 --- V0 Intrinsic V(0) magnitude number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 mag MV Absolute V magnitude number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 mag DistMod Distance modulus V(0)-Mv number= Claria, J. J. 1974, Elementos de Fotometria Estellar, Instituto Venezolano de Astronomia (Merida, Venezuela) Crawford, D. L. 1975, AJ, 80, 955 Crawford, D. L. 1978, AJ, 83, 48 Crawford, D. L. 1979, AJ, 84, 1858 Eggen, O. J. 1974, ApJ, 188, 59 Eggen, O. J. 1981, ApJ, 247, 507 Stromgren, B. 1966, ARA&A, 4, 433 mag Membu Membership indicator from uvbyBeta photometry V(0)-Mv number=1 b Possible binary member of cluster F Probable field object f Possible field object G Probable member of background group M Probable cluster member m Possible cluster member n Possible non-member of cluster or background group --- MembU Membership indicator from UBV analysis of table1 number=1 b Possible binary member of cluster F Probable field object f Possible field object G Probable member of background group M Probable cluster member m Possible cluster member n Possible non-member of cluster or background group --- MK spectral types in NGC 2287 HFMR Identification number --- MKSp Adopted MK type number=1 Spectral types ? uncertain or conflicting criteria; : poor plate; / either range possible or between types given; - between types given; sV spectrum variable; SB2 H lines stronger than standards, broad and strong cores, atypical profiles (see LM). --- MKSp1 MK type from a single plate --- Date Date of observation "DD/MM/YY" Rem Remarks number=2 Key to remarks A. Possible contamination from 1A. B. Poor standards at luminosity class III. C. Possible peculiar Hgamma. D. Hbeta,gamma lines show sharp core, diffuse wings. E. SB2? F. H lines broad; not n? G. H line wings slightly peculiar, luminosity difficult to determine. H. Very poor spectrum, moon contamination? Am? I. possible rotational broadening? sV? J. H lines ~ A0; weak G band, metal lines. K. Ca very strong; H lines peculiar. L. Could be III; very poor spectrum. M. H profiles square -> SB2? N. Poor luminosity standards; adopted LM type. O. H lines diffuse but no sharp core. P. Could be double not rotation. Q. H lines sharp; He4026 present. R. H lines broad; weak CaK, no He4026. S. Spectra for this star definitely different from each other. T. Hgamma,delta peculiar? U. Luminosity difficult to determine. V. Hgamma,delta double, CaK broad. W. Both CaK and He4026 present. X. Possible Ap or composite. Y. Hbeta,epsilon suggest n? Z. Possible composite? a. Possible weak Si4128. b. Standards poor; definitely more luminous than IIIb. c. Possible He4026? d. Possible square profiles. e. Either composite or shell. f. Spectra slightly different. g. A star appears stronger in 1981 exposure. h. Adopted LM type. i. He weak? j. CaK sharper than H lines? k. Hint of TiII 3993? --- MKSp2 Other MK type --- Ref References. The notation "[2]" indicates that the spectral type is for both stars in the pair number=3 References C Cox, A. N. 1954, ApJ, 119, 188 H Hartoog, M. R. 1976, AJ, 205, 807 LG Levato, H., & Garcia, B. 1984, ApJ, 24, L161 LM Levato, H., & Malaroda, S. 1979, PASP, 91, 636 RHH van Rensbergen, W., Hammerschlag-Hensberge, G., & van den Heuvel, E. P. J. 1978, A&A, 64, 131 S Sowell, J. R. 1987, ApJS, 64, 241 --- macros.tex macros for the tables in TeX table1a.tex TeX version of table1 (left part) table1b.tex TeX version of table1 (right part) table2.tex TeX version of table2 table4.tex TeX version of table4 Patricia Bauer CDS 1994 Sep 16 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_1533.xml The intermediate age open cluster NGC 7044. J/AJ/106/1547 J/AJ/106/1547 NGC 7044 The intermediate age open cluster NGC 7044. A Aparicio E J Alfaro A J Delgado J A Rodriguez-Ulloa J Cabrera-Cano Astron. J. 106 1547 1993 1993AJ....106.1547A Clusters, open Photometry, UBVRI Photometry is presented for the open cluster NGC 7044, based on Johnson-Cousins UBVR CCD photometry of 896 stars in a region of 4'20"x4'20" in the cluster field.
Photometrical data of NGC 7044 Number Identification number of each star --- X Position (0.254"/pix) pix Y Position (0.254"/pix) pix (U-B) color index mag e_U Mean error on U, as given by ALLSTAR mag (B-V) color index mag e_B Mean error on B, as given by ALLSTAR mag V V magnitude mag e_V Mean error on V, as given by ALLSTAR mag (V-R) color index mag e_R Mean error on R, as given by ALLSTAR mag Francois Ochsenbein CDS 1994 Apr 25 Antonio Aparicio <aaj@ll.iac.es> J_AJ_106_1547.xml Hubble Space Telescope / Faint Object Camera observations of the inner regions of the galactic globular cluster M15. J/AJ/106/154 J/AJ/106/154 HST Observations in inner region of M15 Hubble Space Telescope / Faint Object Camera observations of the inner regions of the galactic globular cluster M15. F R Ferraro F Paresce Astron. J. 106 154 1993 1993AJ....106..154F Clusters, globular Photometry, ultraviolet Stars, variable A set of high resolution images of the core of the Galactic Globular Cluster M15 (NGC 7078) were obtained for the first time with the Faint Object Camera on Hubble Space Telescope through the f/48-F140W, f/48-F220W and f/96-F342W ultraviolet filters. Out of these, 19 are variables discovered from the rms frame-to-frame scatter of the F220W images, 14 of which are probably RR Lyrae.
Non-variable stars in the observed field Name Star sequence number --- m140 Magnitude at 140 nm mag m220 Magnitude at 220 nm mag m342 Magnitude at 340 nm mag X X coordinate pix Y Y coordinate pix Variable stars in the observed field Vname Variable star sequence number --- Type Star type --- m140 Magnitude at 140 nm mag m220 Magnitude at 220 nm mag m342 Magnitude at 340 nm mag X X coordinate pix Y Y coordinate pix Candidate Blue Stragglers stars in M15 BSname Blue Stragglers candidate sequence number --- Name Star sequence number of table1 --- m220 Magnitude at 220 nm mag m220-m342 Color index mag Francois Ochsenbein, Patricia Bauer CDS 1994 Jul 05 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_106_154.xml ICCD speckle observations of binary stars. X. A further survey for duplicity among the bright stars J/AJ/106/1639 J/AJ/106/1639 ICCD speckle observations of binary stars. X. ICCD speckle observations of binary stars. X. A further survey for duplicity among the bright stars H A Mcalister B D Mason W I Hartkopf M M Shara Astron. J. 106 1639 1993 1993AJ....106.1639M Interferometry Stars, double and multiple Speckle interferometric observations from the Canada-France-Hawaii 3.6 m and Cerro Tololo 4 m telescopes are reported for 1123 stars selected from the Yale Bright Star Catalogue in a continuing effort to detect new binaries among the bright stars. Thirty-two previously unresolved binaries have been detected, including companions to Xi UMa and 15 S Mon. Measures of 107 previously resolved systems, many of which resulted from earlier speckle observations, are also presented.
Measurements of new binaries Measurements of known binaries Observational history of new bright star binaries WDS Epoch 2000.0 coordinates used as designator in the Washington Double Star Catalogue maintained by Charles Worley at the U. S. Naval Observatory (hhmmmSddmm). --- HR Harvard Revised (HR) number --- CHARA Newly assigned CHARA discovery number (table1 and table7 only) --- Discov Discovered (table2 only) --- V Visual magnitude from the Bright Star Catalogue (BSC; Hoffleit, D. 1982, Yale University Observatory, New Haven) mag n_V Visual magnitude code (1) ' ' = V on UBV (Johnson) system 'R' = HR magnitudes reduced to the UBV system 'H' = original HR magnitude --- Sp MK spectral type from BSC --- n Number of components, N, from the BSC and incremented to reflect the new companions (table1 only) --- Obs Epoch of the observation as the fraction of the Besselian year yr PA Position angle of new measurement deg Sep Angular separation of new measurement arcsec Ref Reference number (2) (table7 only) --- Negative results from CFHT Negative results from CTIO HR HR number from the BSC number= Footnotes: Also found to be single in: (1) McAlister (1978, PASP, 90, 288) (2) McAlister & Hendry (1981, PASP, 93, 221) (3) Hartkopf & McAlister (1984, PASP, 96, 105) (4) McAlister et al. (1987a, AJ, 92, 183) (BSS1) (5) Lu et al. (1987, AJ, 94, 1318) (6) McAlister et al. (1989, AJ, 97, 510) (BSS2) (7) Mason et al. (1993, AJ, 106, 637) (8) Table 4 (9) Table 3 --- note Footnotes separated by comma and enclosed in parentheses number= Footnotes: Also found to be single in: (1) McAlister (1978, PASP, 90, 288) (2) McAlister & Hendry (1981, PASP, 93, 221) (3) Hartkopf & McAlister (1984, PASP, 96, 105) (4) McAlister et al. (1987a, AJ, 92, 183) (BSS1) (5) Lu et al. (1987, AJ, 94, 1318) (6) McAlister et al. (1989, AJ, 97, 510) (BSS2) (7) Mason et al. (1993, AJ, 106, 637) (8) Table 4 (9) Table 3 --- Unresolved speckle binaries HR HR number from the BSC --- Name Name --- note Reference number number=1 Reference numbers: 1) McAlister & Hartkopf (1988, Second Catalog of Interferometric Measurements of Binary Stars, CHARA Contribution No. 2, Georgia State University) 2) Weigelt & Wirnitzer (1983, Opt. Lett., 8, 389) 3) McAlister et al. (1992, AJ, 104, 810) 4) Isobe et al. (1990, Publ. Natl. Astron. Obs. Japan 1, 217) --- Meas Number of measurements --- Neg Number of negative measurements --- Comment Comments --- Apparently spurious binaries WDS Epoch 2000.0 coordinates used as designator in the Washington Double Star Catalogue maintained by Charles Worley at the U. S. Naval Observatory (hhmmmSddmm). --- HR HR number from the BSC --- CHARA CHARA number --- O_Discov "Discovery" epoch yr PA Position angle, theta deg Sep Angular separation, rho arcsec Nconf Number of attempted confirmations --- Confmin Duration of confirmation attempts, minimum yr Confmax Duration of confirmation attempts, maximum yr Preliminary orbital elements HR HR number from the BSC --- P Period yr a Semi-major axis arcsec i Inclination deg OMEGA Longitude of ascending node deg T Epoch yr e Eccentricity --- omega Longitude of perihelion deg Patricia Bauer CDS 1994 Jun 27 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_1639.xml CCD photometry of the old open cluster M67 J/AJ/106/181 J/AJ/106/181 CCD photometry of open cluster M67 CCD photometry of the old open cluster M67 K A Montgomery L A Marschall K A Janes Astron. J. 106 181 1993 1993AJ....106..181M Clusters, open Photometry, UBV UBV photometry is presented for stars in the open cluster M67.
Photometry in M67 MMJ Star number in M67 --- n_MMJ Note as ) = bright star * = star which falls on the photometric binary sequence in the color-magnitude diagram --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Vmag on Johnson system mag B-V Color mag U-B ? mag V-R ? mag V-I ? mag e_Vmag Mean error on V mag e_(B-V) Mean error on B-V mag e_(U-B) Mean error on U-B mag e_(V-R) Mean error on V-R mag e_(V-I) Mean error on V-I mag e_pos Mean error on the position pix o_V Number of observations on V --- o_(B-V) Number of observations on B-V --- o_(U-B) Number of observations on U-B --- o_(V-R) Number of observations on V-R --- o_(V-I) Number of observations on V-I --- Refs Cross-references number=1 the first number corresponds to Sanders (1977, A & AS, 27, 89) numbers preceded with a roman numeral are from Eggen and Sandage (1964, ApJ, 140, 130) numbers preceded with an F are from Fagerholm (1906) numbers preceded with a G refer to Gilliland et al. (1991, AJ, 101, 541) and the table 4 reference is to stars brighter than 12th magnitude with the source of the photometry given in table 4. --- Bright stars MMJ Star number in M67 --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec V on Johnson system mag B-V Color mag V-I ? mag r_BVI Source of photometry: ES is Eggen and Sandage (ApJ, 140, 130) JS is Janes and Smith (AJ, 89, 487) G is Gilliland et al. (AJ, 101, 541), M is Murray et al. (Roy. Obs. Bull. No. 91) S is Sanders (RMxA, 17, 31). --- Sanders Sanders' number (A&AS 27, 89) --- Sanders to MMJ cross-identification Sanders' number (A&AS 27, 89) --- MMJ number as in Table 3 --- Francois Ochsenbein CDS 1993 Dec 22 UNKNOWN UNKNOWN The declination of star MMJ 6470 (tables 3 and 4) was corrected (communication with Kent Montgomery, kent@hyades.bu.edu) Courtesy Kent Montgomery. J_AJ_106_181.xml Early-type stars in orthogonal halo fields. II. Identification of metal-rich A stars in the halo J/AJ/106/1839 J/AJ/106/1839 Metal-rich halo A stars Early-type stars in orthogonal halo fields. II. Identification of metal-rich A stars in the halo A W Rodgers W H Roberts Astron. J. 106 1839 1993 1993AJ....106.1839R J/AJ/106/591 : OP Survey of Halo early-type stars (Rodgers+ 1993) Rodgers A.W. & Roberts W.H., Paper III. =1993AJ....106.2294R Equivalent widths Radial velocities Stars, early-type The results of spectrophotometry of the Ca II K and Balmer lines and radial velocity measurements for stars earlier than type F0, with 10<V<15.5 in fields at (l;b)=(90deg, 270deg; -45deg) are reported. Slit spectroscopy of 320 stars shows that in this magnitude range there are ~80 stars with [Fe/H]>-0.5. The metal-rich population has a vertical scale height of ~600pc and a space density at the Sun equal to 1/225 of the young thin disk A star population. The metal-rich A stars have V_rot_=210+/-60km/s with decreasing angular momentum as a function of distance from the Galactic plane. The line-of-sight velocity dispersion is 40+/-3km/s indicating an anomalous relation between structure and kinematics. There is strong evidence that these stars are identical in properties to the metal-rich extended populations found by Perry [1969AJ.....74..139P] at the NGP and Rodgers [1971ApJ...165..581R] at the SGP.
Spectrophotometry and radial velocities of stars classified as of type earlier than F0 in the fields (l;b)=(90 deg, 270 deg; -45 deg) from the catalog of Paper I Name Object identifier --- EWK Equivalent width of Ca II K 0.1nm EWHd Equivalent width of Ca II Hdelta 0.1nm RV Radial velocity rel. to Local Std. of Rest The following corrections were adopted: for l=90 deg; b=-45 deg, V_lsr=V_helio+6km/s for l=270 deg; b=-45 deg, V_lsr=V_helio-16km/s km/s GLON Galactic latitude deg GLAT Galactic longitude deg CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 19-Feb-1996 J_AJ_106_1839.xml NGC 6611: A Cluster Caught in the Act J/AJ/106/1906 J/AJ/106/1906 NGC 6611: A Cluster Caught in the Act NGC 6611: A Cluster Caught in the Act L A Hillenbrand P Massey S E Strom K M Merrill Astron. J. 106 1906 1993 1993AJ....106.1906H Clusters, galaxy Photometry Spectroscopy This catalog is the RA-sorted list of astrometry and optical/infrared photometry for optically visible sources in NGC 6611 (aka M8, The Eagle Nebula). All positions are for the epoch J2000. We have combined optical CCD photometry and spectroscopy with infrared imaging photometry to study the young cluster NGC 6611. We use these data to derive improved values for the reddening law (R=3.75) and the distance modulus (m-M=11.5), and to construct a physical H-R diagram from which we can probe the ages, masses, and evolutionary states of this stellar ensemble. The H-R diagram shows a strong population of high-mass stars, the most massive of which has a mass of roughly 80 solar masses, similar to what we find in other Galactic and Magellanic Cloud clusters and associations. The age of the massive stellar population in NGC 6611 is approximately 2 million years, with an age spread of, perhaps, a million years, although the data are also consistent with there being no discernible age spread among the most massive stars. However, the H-R diagram does reveal that one star of somewhat lower mass (30 solar masses) must have formed approximately 6 million years ago. The upper end of the mass function of NGC 6611 is found to have a slope of Gamma=-1.1 +/- 0.3, indistinguishable from a Salpeter slope, and similar to what we have found in other Galactic associations, but shallower than what we have found in the Magellanic Clouds. Our most significant result, however, is that we catch this cluster in the act of forming intermediate mass (3-8 Solar masses) stars. This is the first well-established case where large numbers of intermediate-mass stars have been seen on their way to the zero-age main sequence. That intermediate mass pre-main sequence stars are indeed present is evidenced both by their location above the zero-age main sequence in the H-R diagram, and in some cases by their spectroscopic and infrared signatures of (possibly remnant protostellar) circumstellar material. The pre-main sequence population ranges from as young as 0.25 million years to at least 1 million years of age. We find an highly unusual number (27) of emission-line stars, which appear quite similar in their optical and infrared continuum and optical spectroscopic properties to ``classical Be/Ae" stars (as opposed to Herbig Be/Ae stars). Our data are inconsistent with the traditional interpretation that these "classical Be/Ae" stars are slightly evolved stars undergoing mass loss. Instead, we offer the conjecture that these may be young stars whose circumstellar disks have become optically thin, and produce Balmer emission lines. The infrared data do indicate a number of stars, particularly amongst the embedded sample, whose colors are consistent with those of stars thought to be surrounded by optically thick circumstellar accretion disks. The identification of such disks around young massive stars continues to be rare, and implies that the disk survival times around intermediate and high mass stars are much shorter (< 0.5 myr) than those of disks surrounding lower mass stars.
NGC 6611 Optical and Near-Infrared Photometry Data n_ID emission line object flag --- ID previous identification number See paper text for explanation of ID. --- RAh J2000 hours of right ascension h c field separator --- RAm minutes of right ascension min c field separator --- RAs seconds of right ascension s DE- sign of declination --- DEd J2000 degrees of declination deg c field separator --- DEm minutes of declination arcmin c field separator --- DEs seconds of declination arcsec V V magnitude mag u_V uncertainty flag in V --- B_V B-V color mag u_B_V uncertainty flag in B-V --- U_B U-B color mag u_U_B uncertainty flag in U-B --- K K magnitude mag u_K uncertainty flag in K --- H-K H-K color mag u_H-K uncertainty flag in H-K --- J-H J-H color mag u_J-H uncertainty flag in J-K --- V-K V-K color mag N. Paul M. Kuin NSSDC/ADC 1994 Jul 28 J_AJ_106_1906.xml A photometric investigation of the eclipsing binary V505 Sagittarii. J/AJ/106/2058 J/AJ/106/2058 Karle observations of V505 Sgr A photometric investigation of the eclipsing binary V505 Sagittarii. C R Chambliss R L Walker J H Karle H B Snodgrass Y A Vracko Astron. J. 106 2058 1993 1993AJ....106.2058C Binaries, eclipsing Stars, variable Karle observations of V505 Sgr The table contains a listing of 1074 observations of V505 Sagittarii which were made by Karle during 29 nights in 1960 and 1961 with a 25-cm reflector at the Lewis and Clark College in Portland, Oregon. An RCA 1P21 photomultiplier was used, and the comparison star was HD 187664. The observations were unfiltered, and C.R. Chambliss and R.L. Walker have estimated the effective wavelength to be 4600A. These observations were not corrected for differential extinction. The reductions for time and for delta-magnitude were made by Yura Vracko in 1990. Karle observed nine times of primary minimum light and one time of secondary minimum. These were determined by Chambliss and Walker using the method of Kwee and van Woerden (1956), and they are listed in the printed paper. A least squares solution for these times of minimum light yielded the following ephemeris: T(min) = JD 2437108.8818 + 1.1828637 E. This ephemeris has been used to calculate the phases and phase angles which appear in this table. V505 Sgr is a classical Algol system consisting of an A2 V primary and a G5 IV secondary that fills its Roche lobe. New times of minimum light are presented. The period of the eclipsing system (1.18287d) varies, due in part to an orbital light-time effect. A third component has been detected that orbits the eclipsing pair. This investigation uses the SIMPLEX algorithm [Kallrath & Linnell, ApJ, 313, 346 (1987)] and the Differential Correction code [Wilson, ApJ, 234, 1054 (1979)] to analyze two separate datasets. The results indicate the third component, an F8 V star, contributes about 5% of the light to the system. The minimum projected distance between the third component and the eclipsing pair is 37 AU. This implies an orbital period of about 105 years, a value that differs with the O-C data. The photometric solution, combined with recent spectroscopic data, yields R(1)=2.14R(Sun) and R(2)=2.24R(Sun) and M(1)=2.20M(Sun) and M(2)=1.15M(Sun).
V505 Sgr HD 187949 HR 7571 19 53 06.3 -14 36 08
Karle observations of V505 Sgr HJD Heliocentric Julian Date d Phase Phase --- Angle Phase angle deg Delta Delta magnitude mag CDS 1996 Feb 21 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_2058.xml New limb-darkening coefficients for modeling binary star light curves J/AJ/106/2096 J/AJ/106/2096 New limb-darkening coefficients for modeling New limb-darkening coefficients for modeling binary star light curves W Van Hamme Astron. J. 106 2096 1993 1993AJ....106.2096V Models, atmospheric Stars, binary Monochromatic, passband-specific, and bolometric limb-darkening coefficients for a linear as well as nonlinear logarithmic and square root limb-darkening laws are presented. The calculations are based on the most recent ATLAS stellar atmosphere models for solar chemical composition stars with a wide range of effective temperatures and surface gravities.
Bolometric limb-darkening coefficients Model Model number --- Teff Effective temperature K log(g) Logarithm of the surface gravity cm/s2 xBol Bolometric linear limb-darkening coefficient x --- QBol Quality factor --- xLog Logarithmic law x coefficient --- yLog Logarithmic law y coefficient --- QLog Quality factor --- xSqu Square root law x coefficient --- ySqu Square root law y coefficient --- QSqu Quality factor --- Passband-specific limb-darkening coefficients Model Model number --- Teff Effective temperature K log(g) Logarithm of the surface gravity cm/s2 Pass Passband --- xLin Linear limb-darkening coefficient --- QLin Quality factor --- xLog Logarithmic law x coefficient --- yLog Logarithmic law y coefficient --- QLog Quality factor --- xSqu Square root law x coefficient --- ySqu Square root law y coefficient --- QSqu Quality factor --- Models parameters Model Model number --- Teff Effective temperature K log(g) Logarithm of the surface gravity cm/s2 A Abundance (always solar abundance) Sun Vturb Microturbulent velocity km/s l/H Convective parameter --- Bolometric coefficients Monochromatic coefficients Model Model number --- lambda Wavelength nm xBol Linear limb-darkening coefficient --- QBol Quality factor number=1 Quality factor Q defined as (all parameters refer to monochromatic values): Q={sum(for i=1 to 17)[D(mu_i_)-D'(mu_i_)]/(17-m)}1/2 where D(mu) = I(mu)/I(1) D'(mu) = I'(mu)/I'(1) and I(mu) is the theoretical specific intensity I'(mu) is the specific intensity according to the limb-darkening approximation This number may help in choosing which limb-darkening law to use in any particular case --- xLog Logarithmic law x coefficient --- yLog Logarithmic law y coefficient --- QLog Quality factor number=1 Quality factor Q defined as (all parameters refer to monochromatic values): Q={sum(for i=1 to 17)[D(mu_i_)-D'(mu_i_)]/(17-m)}1/2 where D(mu) = I(mu)/I(1) D'(mu) = I'(mu)/I'(1) and I(mu) is the theoretical specific intensity I'(mu) is the specific intensity according to the limb-darkening approximation This number may help in choosing which limb-darkening law to use in any particular case --- xSqu Square root law x coefficient --- ySqu Square root law y coefficient --- QSqu Quality factor number=1 Quality factor Q defined as (all parameters refer to monochromatic values): Q={sum(for i=1 to 17)[D(mu_i_)-D'(mu_i_)]/(17-m)}1/2 where D(mu) = I(mu)/I(1) D'(mu) = I'(mu)/I'(1) and I(mu) is the theoretical specific intensity I'(mu) is the specific intensity according to the limb-darkening approximation This number may help in choosing which limb-darkening law to use in any particular case --- I Intensity, I(lambda, mu=1) mW/m2/sr/nm Patricia Bauer CDS 1994 Jun 30 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_2096.xml Photometric study of the old galactic cluster Be 31 J/AJ/106/220 J/AJ/106/220 Photometric study of old galactic cluster Be 31 Photometric study of the old galactic cluster Be 31 H H Guetter Astron. J. 106 220 1993 1993AJ....106..220G Clusters, open Photometry, Cousins Photometry, Kron Photometry, UBV CCD photometry on the Johnson UBV and on the Kron-Cousins VI systems are presented for 732 stars in and near Be 31, an open cluster located towards the galactic anticenter.
Observational data No Star number --- V V magnitude mag B-V B-V color mag U-B U-B color mag V-I V-I color mag X X coordinate pix Y Y coordinate pix Patricia Bauer CDS 1994 Jun 22 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_220.xml UBV photometry of luminous stars toward the Galactic Center J/AJ/106/2291 J/AJ/106/2291 UBV photometry toward Galactic Center UBV photometry of luminous stars toward the Galactic Center B C Reed Astron. J. 106 2291 1993 1993AJ....106.2291R III/43 : (LSS) Luminous Stars in the Southern Milky Way (Stephenson+ 1971) J/PASP/105/1465 : Distant OB Stars in the Galaxy (Reed 1993) J/ApJS/87/367 : UBV-beta database for LS stars (Reed, 1993) J/ApJS/97/189 : Database for Stephenson-Sanduleak Stars (Reed+ 1995) J/A+AS/117/313 : LSS stars Stroemgren photometry (Reed, 1996) J/AJ/112/2855 : UBV Photometry of LSS stars (Reed+ 1996) J/AJ/113/823 : Radial velocity database for LSS stars (Reed+ 1997) Photometry, UBV UBV photometry of 186 stars with 17h < R.A. < 19h listed in Stephenson and Sanduleak's "Luminous Stars in the Southern Milky Way" catalog (Stephenson C.B. & Sanduleak N. 1971, Publ. Warner and Swasey Obs. 1, No. 1) is reported.
LS stars photometry LSS LS number --- Vmag V magnitude mag B-V B-V color mag U-B U-B color mag e_Vmag Standard deviation of V magnitude (for stars observed more than once) mag e_B-V Standard deviation of B-V color mag e_U-B Standard deviation of U-B color mag Nobs Number of times the star was observed --- Note Notes. A '*' designates stars that were observed at the telescope to have one or more faint nearby companions; in most cases these should not significantly affect the results. Spectral information is reproduced directly from the LSS catalog. Somewhat arbitrarily, stars with e_V > 0.05 mag have been flagged as possibly variable. --- Patricia Bauer CDS 1994 Jun 27 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_2291.xml The Behlen Observatory variable star survey: finding charts and light curves for the first ninety-three stars J/AJ/106/2429 J/AJ/106/2429 Behlen Obs. variables stars survey The Behlen Observatory variable star survey: finding charts and light curves for the first ninety-three stars E G Schmidt D E Reiswig Astron. J. 106 2429 1993 1993AJ....106.2429S Photometry Stars, variable The table contain the photometric data for the variable stars discussed by Schmidt, A.J. 102, 1766, 1991 and this paper.
Photometric data Name Star name --- HJD Heliocentric Julian Date d Phase the phase calculated with the period and epoch in the extension header --- V V magnitude mag R R magnitude mag V-R V-R color mag Flag Flag, ':' if the variable fell close to a bad pixel or column on the CCD. Such data should be treated with caution. --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 08-Nov-1994 Mar 29 Addresses: Schmidt E.G. eschmidt@unlinfo.unl.edu Behlen Observatory, Department of Physics and Astronomy, University of Nebraska, Lincoln, Nebraska 68588-0111 and The National Science Foundation, 1800 G St. NW, Washington, DC 20550 Reiswig D.E. Behlen Observatory, Department of Physics and Astronomy, University of Nebraska, Lincoln, Nebraska 68588-0111 AAS CD-ROM series, Volume 2, 1994 J_AJ_106_2429.xml A photometric and spectrographic study of SX Phoenicis J/AJ/106/2493 J/AJ/106/2493 Photometry and Spectroscopy of SX Phe A photometric and spectrographic study of SX Phoenicis C Kim D H McNamara C G Christensen Astron. J. 106 2493 1993 1993AJ....106.2493K Photometry, ubvy, beta Radial velocities Stars, variable Simultaneous photometric (uvbyBeta) and spectrographic observations of SX Phe are presented.
uvbyBeta photometry of SX Phoenicis Name Star name, 'SX Phe' or 'COMP' for the comparison star, HD 223011 --- HJD Heliocentric Julian Date d ymag y magnitude mag b-y b-y color mag c1 c1 index mag m1 m1 index mag Beta Beta index mag Radial velocity of SX Phoenicis HJD Heliocentric Julian Date d RV Radial velocity km/s Lee Brotzman ADS 1994, Patricia Bauer [CDS] 18-Oct-1994 Mar 30 Addresses: Kim C. kimastro@garam.kreonet.re.kr Department of Earth Science Education, Chonbuk National University, Korea McNarama D.H. and Christiensen C.G. pasp@astro.byu.edu Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602 AAS CD-ROM series, Volume 2, 1994 J_AJ_106_2493.xml Proper motions in the southern ESO Areas 207, 439, AND 440 J/AJ/106/2575 J/AJ/106/2575 Proper motions in the southern ESO Areas Proper motions in the southern ESO Areas 207, 439, AND 440 M T Ruiz M Y Takamiya R Mindez J Maza M Wishnjewsky Astron. J. 106 2575 1993 1993AJ....106.2575R Proper motions Selected areas Proper motion stars have been identified from red IIIaF ESO Schmidt plates. This catalogue includes stars found in ESO Areas 207, 439, and 440 having mu >= 0.1 arcsec/yr.
ESO areas 207, 439 and 440 (tables 2, 3 and 4) Area ESO area number --- N Running number --- No Star number in Area --- name Other names --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec m(R) Red magnitude mag pm Proper motion arcsec/yr PA Position angle deg table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 table4.tex LaTeX version of table4 Patricia Bauer CDS 1994 Jun 30 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_2575.xml ICCD speckle observations of binary stars. VIII. Measurements during 1989-1991 from the Cerro Tololo 4 m telescope J/AJ/106/352 J/AJ/106/352 ICCD speckle observations of binary stars. VIII. ICCD speckle observations of binary stars. VIII. Measurements during 1989-1991 from the Cerro Tololo 4 m telescope W I Hartkopf B D Mason D J Barry H A McAlister W G Bagnuolo Astron. J. 106 352 1993 1993AJ....106..352H Interferometry Stars, double and multiple One-thousand eighty-eight observations of 947 binary star systems, observed by means of speckle interferometry with the 4 m telescope on Cerro Tololo, are presented. These measurements, made during the period 1989-1991, comprise the second installment of results stemming from the expansion of our speckle program to the southern hemisphere.
Binary star speckle measurements RAh Right Ascension 2000.0 h RAdm Right Ascension 2000.0, (deci-minutes, there is an implicit decimal point between bytes #4 and 5) min DE- Declination sign --- DEd Declination 2000.0 deg DEm Declination 2000.0 arcmin Name ADS, HR, or DM designation (note that this field does not appear in the printed paper) --- Discov Discoverer designation --- HD Henry Draper designation --- BY Besselian year of observation yr PA Position angle deg u_PA Uncertainty flag on position angle --- Sep Angular separation arcsec u_Sep Uncertainty flag on angular separation --- notes1.tex TeX version of notes1 Patricia Bauer CDS 1994 Jun 27 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_352.xml Lick slit spectra of thirty-eight objective prism quasar candidates and low metallicity halo stars J/AJ/106/426 J/AJ/106/426 Lick slit spectra of quasar Lick slit spectra of thirty-eight objective prism quasar candidates and low metallicity halo stars D Tytler X -M Fan V T Junkkarinen R D Cohen Astron. J. 106 426 1993 1993AJ....106..426T Photometry, BV QSOs Spectroscopy We present Lick Observatory slit spectra of 38 objects which were claimed to have pronounced ultraviolet excess and emission lines. Zhan & Chen (ZC) selected these objects by eye from a UK Schmidt telescope IIIaJ objective prism plate of a field at 0h 0.0deg (l ~= 98 deg, b ~= -60 deg). We concentrate on m(J) ~= 18-19 objects which Zhan and Chen (ZC) thought were most likely to be quasistellar objects (QSOs) at redshift z(em) >= 2.8. Most of our spectra have FWHM spectral resolutions of about 4 A, and relatively high S/N of about 10-50, although some have FWHM ~= 15 A or lower S/N. We find eleven QSOs, four galaxies at z ~= 0.1, twenty-two stars and one unidentified object with a low S/N spectrum. The ZC lists are found to contain many QSOs at low z but few at high z, as expected. Of eleven objects which ZC suggested were QSOs with z(prism) <= 2.8, eight (73%) are QSOs. But only three of twenty-five candidates with z(prism) >= 2.8 are QSOs, and only two (8%) of these are at z >= 2.8. Unfortunately, the ZC prism redshifts are often incorrect: only five of the eleven QSOs are at redshifts similar to z(prism). Six of the QSOs show absorption systems, including Q0000+027A with a relatively strong associated C IV absorption system, and Q0008+008 (V ~= 18.9) with a damped Ly alpha system with an HI column density of 10^21 cm^-2. The stars include a wide variety of spectral types. There is one new DA 4 white dwarf at 170 pc, one sdB at 14 kpc, and three M stars. The rest are of types F, G, and K. We have measured the equivalent widths of the Ca II K line, the G band, and the Balmer lines in ten stars with the best spectra, and we derive metallicities. Seven of them are in the range -2.5 <= [Fe/H] <= -1.7, while the others are less metal poor. If the stars are dwarfs, then they are at distances of 1 to 7 kpc, but if they are giants, typical distances will be about 10 kpc.
Journal of observations Name Object designation --- Obs Observation date, U.T. "DD/MM/YY" Int.time Integration time s Setup Instrumental setup (see note (1)) --- lamMin Minimum wavelength of the total range (for setup A and B) 0.1nm lamMax Maximun wavelength of the total range (for setup A and B) 0.1nm lambMin Minimum wavelength of the blue range (for setup C) 0.1nm lambMax Maximun wavelength of the blue range (for setup C) 0.1nm lamrMin Minimum wavelength of the red range (for setup C) 0.1nm lamrMax Maximun wavelength of the red range (for setup C) 0.1nm Ref Zhan and Chen references number=2 ZC1: Zhan Y. & Chen J-S. 1987, AcApSn 7, 99; Trans. in Chin.A.Ap., 11, 191 ZC2: Zhan Y. & Chen J-S. 1987, AcApSn 7, 203; Trans. in Chin.A.Ap., 11, 299 ZC3: Zhan Y. & Chen J-S. 1989, AcApSn 9, 37; Trans. in Chin.A.Ap., 13, 139 ZC4: Zhan Y. & Chen J-S. 1989, AcApSn 9, 147; Trans. in Chin.A.Ap., 13, 321 --- Summary of spectra Name Object designation --- zOP Objective prism redshift from the ZC references (see table1) --- q_zOP Reliability index Q from the ZC references (see note(1)) --- Type Object type (see note (2)) --- Sp1 Spectral type from the spectral features --- Sp2 Spectral type from (B-V)0 --- z Redshift --- u_z Uncertainty flag on z --- lines Spectral lines --- Magnitudes and spectral indices Name Object designation --- Setup Note flag: 'A' for magnitudes measured from Setup A spectrum, and likely to be systematically too faint; 'B' for magnitudes measured from Setup B spectrum. --- B(J) B(J) magnitude from ZC references, obtained from image sizes on a direct Schmidt plate. mag U U magnitude. U is highly uncertain mag B B magnitude. B is highly uncertain mag V V magnitude. V is highly uncertain mag (B-V)0 (B-V)0 color. (B-V)0 is highly uncertain mag (B-V) (B-V) color estimated from the Balmer line index HP using: (B-V)0 = 0.962 - 0.292HP + 0.036HP^2 mag Delta Slit (B-V) minus HP index (B-V) mag HP Balmer line index HP, where HP = -0.120 + 0.5Halpha + 0.555Hgamma, which is the average of the measured equivalent width of Halpha, and an estimate of that width based on the measured equivalent width of Hgamma. 0.1nm KP Index KP', the Ca II K equivalent width measured in the 18 A interval, corrected for interstellar Ca II K absorption by subtracting 0.22 A. 0.1nm GP G-band (CH) index, GP, the equivalent width in the 15 A band around 4300 A. 0.1nm Emission lines Name Object designation --- <z(em)> Mean emission redshift --- Ion Ion --- lamLab Laboratory vacuum wavelength 0.1nm u_lamLab Uncertainty flag on lamLab --- lamObs Observed wavelength 0.1nm EWobs Observed frame equivalent width. All values have a decimal point, so that they will be read correctly by a computer program, but some of the values were originally integers 0.1nm z(em) Emission redshift --- Com Comments. The comment 'see notes' refers to file notes --- Major absorption lines in the QSO spectra Name Object designation --- No Sequential number counting the line for this object --- WObs Observed vacuum wavelength 0.1nm n_WObs When 'd', it means that the line was seen by reference ZC2 (see table1 description) --- EWobs Observed equivalent width 0.1nm Ident Line identification --- WLab Laboratory wavelength 0.1nm n_WLab Note flags: 'b' Blended with C IV (1550 A) 'c' see notes file --- z(abs) Absorption redshift --- tables.tex TeX version of the tables Patricia Bauer CDS 1994 Jul 25 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_426.xml Metal abundances for a large sample of globular clusters in M87 J/AJ/106/493 J/AJ/106/493 Globular clusters in M87 Metal abundances for a large sample of globular clusters in M87 M G Lee D Geisler Astron. J. 106 493 1993 1993AJ....106..493L Clusters, globular Galaxies, optical Photometry, CMT1T2V We present deep integrated Washington CCD photometry of the extremely populous globular cluster system of NGC 4486 (M87) in Virgo. The metallicities of 407 of the best candidates with T1 < 22 have been estimated from the (C-T1) color. These values are internally precise to ~0.15dex and accurate to ~0.25dex. The mean metallicity of the globular clusters is [Fe/H] = -0.86dex, with a formal standard error of the mean of 0.03dex but a more realistic uncertainty of about 0.2dex. This value is higher than that of the corresponding means of the globular clusters in the Galaxy and M31, but similar to those of the globular clusters in NGC 1399 and NGC 5128, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for the globular clusters in NGC 1399 and NGC 5128. As found by Couture et al. [ApJS, 73, 671 (1990)], there is a large metallicity dispersion at any radius, with a sigma ~ 0.65dex. However, in contrast to their result and that of previous small-field CCD studies, the globular clusters display a marked gradient in both mean (M-T1) and (C-T1) color with galactocentric distance. The mean metallicity decreases by some 0.6dex over the radial extent of the cluster sample. This result is consistent with the early photographic study by Strom et al. [ApJ, 245, 416 (1981)]. The metallicity distribution function is remarkably similar to that of NGC 1399 found by Ostrov et al. [AJ, 105, 1762 (1993)] using the same technique. The two central cluster ellipticals show significant peaks at very similar metallicities, indicating similar formation and enrichment histories. We also find that this structure in the metallicity distribution function persists to radii where the halo light is dominated by the cD envelope.
M87 globular cluster candidates with T1 < 21 Field Field designator: N1 = North, E1 = East-1, E2 = East-2, W1 = West, and C = Center. --- ID Running number (finding charts are given in Plates 15-19 in the printed paper. --- X X coordinate of object pix Y Y coordinate of object pix T1 T1 magnitude (Washington system) mag e_T1 rms uncertainty on T1 mag M-T1 M-T1 color (Washington system) mag e_M-T1 rms uncertainty on M-T1 mag C-T1 C-T1 color (Washington system) mag e_C-T1 rms uncertainty on C-T1 mag [Fe/H] Derived metal abundance, [Fe/H] --- RG Projected galactocentric distance arcsec Patricia Bauer CDS 1994 Sep 20 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_493.xml The small scale environment of low surface brightness disk galaxies J/AJ/106/530 J/AJ/106/530 Low surface brightness disk galaxies The small scale environment of low surface brightness disk galaxies G D Bothun J M Schombert C D Impey D Sprayberry S S McGaugh Astron. J. 106 530 1993 1993AJ....106..530B Galaxies A sample of approximately 340 low surface brightness (LSB) disk galaxies with measured redshifts was used in combination with the Center for Astrophysics redshift survey to test the hypothesis that LSB galaxies have a deficit of nearby companion galaxies compared to high surface brightness (HSB) disk galaxies. This catalog lists the galaxies found near each galaxy and its distance from the central galaxy.
Summary of Counts Sample Sample designation --- Vrange Velocity range km/s RadProj Projected radius out to which the counts were made Mpc Ngal Number of galaxies forming the sample mean --- Nrej Number of rejected galaxies --- <N> Sample mean. In general, mean quantities are calculated after one cycle of 2.5 sigma projection. --- e_<N> rms uncertainty in sample mean. --- *Difference in mean counts Sample Sample designation --- Vrange Velocity range km/s POSS5 POSS comparison at 0.5 Mpc radius --- POSS5B POSS at 0.5 Mpc obtained by considering subset B in comparison to the POSS HSB sample --- POSS10 POSS comparison at 1.0 Mpc radius --- POSS10B POSS at 1.0 Mpc considering subset B --- POSS15 POSS comparison at 1.5 Mpc radius --- POSS15B POSS at 1.5 Mpc considering subset B --- POSS20 POSS comparison at 2.0 Mpc radius --- POSS20B POSS at 2.0 Mpc considering subset B --- APM5 APM comparison at 0.5 Mpc radius --- APM10 APM comparison at 1.0 Mpc radius --- APM15 APM comparison at 1.5 Mpc radius --- APM20 APM comparison at 2.0 Mpc radius --- Nearest-neighbor summary Sample Sample designation --- Ngal Number of galaxies which have at least one companion within a projected radius of 2.0 Mpc --- Vrange Velocity range km/s Dist Mean projected distance to the nearest companion Mpc e_Dist rms uncertainty on mean projected distance Mpc DmaxPOSS KS statistic, Dmax, for the POSS sample --- cl_DmaxPOSS Confidence level that Dmax exceeds --- DamxAPN KS statistic, Dmax, for the APM sample --- cl_DmaxAPM Confidence level that Dmax exceeds --- The most isolated LSB galaxies Name Galaxy name --- Sample Sample designation (POSS or APM) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Vel Velocity km/s Com Comments --- The most popular LSB galaxies Name Galaxy name --- Sample Sample designation (POSS or APM) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Vel Velocity km/s BrightGal Name of the brightest galaxy within 2 Mpc or a known structure near the galaxy --- Com Comments --- tables.tex Tex version of the tables format.tex Format for tables.tex Patricia Bauer CDS 1994 Jul 25 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_530.xml Statistics and properties of HII regions in NGC 6814 J/AJ/106/56 J/AJ/106/56 HII regions in NGC 6814 Statistics and properties of HII regions in NGC 6814 J H Knapen N Arnth-Jensen J Cepa J E Beckman Astron. J. 106 56 1993 1993AJ....106...56K Galaxies H II regions We present a new Halpha image of high quality of the grand-design galaxy NGC 6814, and describe statistical properties of the HII region population. We have determined positions, angular sizes, and calibrated fluxes of 735 individual HII regions.
HII regions. This table lists the 735 HII regions catalogued in the disk of the grand-design spiral galaxy NGC 6814, using a new H alpha image. The center is also included in the list. ID Identification number of the HII region. HII regions closely grouped in the galaxy have generally closely grouped numbers. --- dRA Right ascension offset from the nucleus. Not corrected for inclination of the galaxy. arcsec dDE Declination offset from the nucleus. arcsec Dist Deprojected distance from the center. An inclination angle of 20 degrees and a position angle of PA=167 degrees were used for the deprojection. arcsec DHII Diameter of the HII region arcsec log(LHII) HII region total integrated luminosity 10-7J/s THII Type assigment given to the HII region. See note number=1 C: center (not an HII region, but included for comparison) A: Arm HII region I: interarm O: outer HII region An outer HII region is defined as lying outside the area of the strong spiral arms, d>43 arcsec or 0.4 R25. --- Patricia Bauer CDS 1994 Jul 25 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_56.xml Early-type stars in orthogonal halo fields. I. An objective-prism survey J/AJ/106/591 J/AJ/106/591 OP Survey of Halo early-type stars Early-type stars in orthogonal halo fields. I. An objective-prism survey A W Rodgers W H Roberts I Walker Astron. J. 106 591 1993 1993AJ....106..591R J/AJ/106/1839 : Metal-rich halo A stars (Paper II.) (Rodgers+ 1993) Rodgers A.W. & Roberts W.H., Paper III. =1993AJ....106.2294R Photometry Spectroscopy The results are reported of an objective-prism survey of stars, mostly earlier than spectral type F5, for two fields at (l;b) = (90 deg and 270 deg; -45 deg). The fields, each of approximately 70 square degrees, are examined on plates taken with the Schmidt Telescope of the Anglo-Australian Observatory. The brightness range of the stars classified is 10 < V < 15. The prism combination used provides a dispersion of 600 A/mm at Hgamma. The spectral classification presented is defined by the equality of equivalent widths of Ca II K and Hdelta at type "F0" and the absence of Ca II K in stars with significant Balmer lines at type "A0". Positions listed in the catalog were measured on the Stromlo PDS microdensitometer.
Catalog of early-type stars Object Object identifier --- RAh Right Ascension J2000.0 h RAm Right Ascension J2000.0 min RAs Right Ascension J2000.0 s DE- Declination sign --- DEd Declination J2000.0 deg DEm Declination J2000.0 arcmin DEs Declination J2000.0 arcsec Sp Spectral type --- Vmag magnitude mag Comment Comments and other designations --- Patricia Bauer CDS 1994 Jun 27 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_591.xml The globular cluster NGC 6366: its blue stragglers and variable stars J/AJ/106/604 J/AJ/106/604 The globular cluster NGC 6366: its blue stragglers The globular cluster NGC 6366: its blue stragglers and variable stars H C Harris Astron. J. 106 604 1993 1993AJ....106..604H Clusters, globular Photometry, BV The nearby, metal-rich, halo globular cluster NGC 6366 has been observed in order to obtain its color-magnitude diagram and to search for variable stars. The color-magnitude diagram indicates that the cluster has a reddening E(B-V) of 0.80 (higher than most previous determinations) and a distance of 3.0kpc. The cluster has numerous blue straggler stars.
Stars in NGC 6366 with R<8arcmin and V<17 ID star ID number --- X position of the star from the cluster center, increases to East pix Y position of the star from the cluster center, increases to North pix V V magnitude mag B-V color index mag Francois Ochsenbein CDS 1994 Feb 25 Hugh C. Harris <hch@nofs.navy.mil> J_AJ_106_604.xml ICCD speckle observations of binary stars. IX. A duplicity survey of the Pleiades, Praesepe, and IC 4665 clusters J/AJ/106/637 J/AJ/106/637 ICCD speckle observations. IX ICCD speckle observations of binary stars. IX. A duplicity survey of the Pleiades, Praesepe, and IC 4665 clusters B D Mason W I Hartkopf H A McAlister J R Sowell Astron. J. 106 637 1993 1993AJ....106..637M Clusters, open Interferometry Stars, double and multiple In order to expand the sample of cluster binaries with potentially short period visual orbits, a speckle survey of 45 Pleiades, 54 Praesepe, and 22 IC 4665 bright stars (V < 10) for possible multiplicity was conducted at the KPNO 4 m Mayall telescope between 1987 October and 1991 November. Of these, three new binaries have been discovered: one in the Pleiades where the new component may be spectroscopic, another in Praesepe which has been confirmed from examinations of archival observations and also has been resolved by occultation, and the third in IC 4665.
Negative results Name Star name (see notes (1)) --- HD Henry Draper number --- Ep1 First epoch of observation yr Ep2 Second epoch of observation yr Patricia Bauer CDS 1994 Jul 25 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_637.xml Dust emission features in 3 micron spectra of Herbig Ae/Be stars J/AJ/106/656 J/AJ/106/656 Herbig Ae/Be stars Dust emission features in 3 micron spectra of Herbig Ae/Be stars T Y Brooke A T Tokunaga S E Strom Astron. J. 106 656 1993 1993AJ....106..656B Equivalent widths Photometry Photometry, infrared Stars, emission Stars, pre-main sequence Low and medium resolution spectra in the 3 micron region were obtained of 24 Herbig Ae/Be stars in a search for organic features from the dust around young stars. The 3.29 micron emission feature from aromatic hydrocarbons was detected for the first time in three objects, Lk Halpha 25, XY Per, and AS 310. Two other stars, HD 245185 and HK Ori may have weak features. Also given are V magnitudes, estimated spectral types, and the extinction for each star.
Summary of 3 {mu}m spectral data of Herbig Ae/Be stars Note Nature of the data number=1 Nature of the data 1 = 3.29 m feature 2 = 3.29 m feature in reflection nebula 3 = Possible 3.29 m feature 4 = No 3.29 m feature detected but IRAS LRS 7.7 and 11.3 micron features 5 = No 3 m spectra but IRAS LRS 7.7 and 11.3 micron features 6 = No 3.29 m feature detected (this work) --- Name Object name --- Sp Estimated spectral type --- n_Av For Elias 1, the visual extinction is given as a range (6-10). n_Av contains '6-' --- Av Estimated visual extinction. For Elias 1, see n_Av mag Dist Estimated distance pc Vmag Visual magnitude mag l_W3.29 Limit flag on W3.29 --- W3.29 Emission equivalent width of the 3.29 micron feature, W3.29 0.1nm e_W3.29 rms uncertainty on W3.29 0.1nm l_F3.29Obs Limit flag on F3.29Obs --- F3.29Obs Observed flux in the 3.29 micron feature, F3.29 10-15W/m2 e_F3.29Obs rms uncertainty on F3.29 10-15W/m2 Rap1 Radius of the aperture, Rap, in arcsec arcsec Rap2 Radius of the aperture, Rap, in AU AU l_F3.29Tot Limit flag on F3.29Tot --- F3.29Tot Estimated total flux of the 3.29 micron feature, F3.29(tot) 10-15W/m2 l_Rext1 Limit flag on Rext --- Rext1 Radius over which the feature is or is not significantly extended. If this field is blank, bytes 85-89 contain estimated values in AU (see text of printed paper). arcsec Rext2 Radius over which the feature is or is not significantly extended. If bytes 79-82 are blank, this is an estimated values. AU l_R3.29 Limit flag on R3.29 --- R3.29 Ratio of total flux in the 3.29 micron feature to the integrated ultraviolet flux of the star after correction for extinction 10-4 l_Narom Limit flag on Narom --- Narom Estimate of relative numbers of aromatics in optically thin limit (see text) 10+2AU+2 Harom High end of range of numbers of aromatics, for one object only, HD 97048 10+2AU+2 Ffir Integrated far-infrared flux estimated from blackbody fits (times 1/lambda = emissivity) to far-infrared photometry (see text) 10-13W/m2 l_Aarom Limit flag on Aarom --- Aarom Estimate of relative abundance of aromatics (see text) --- Ref Reference flags (A-P) number=2 References A) Aitken and Roche 1981, MNRAS, 196, 39 B) Allen et al. 1982, MNRAS, 199, 1017 C) Baas et al. 1983, ApJ, 265, 290 D) Chen and Graham 1993, ApJ (in press) E) Cohen 1975, MNRAS, 173, 279 F) Jourdain de Muizon et al. 1990b, A&A, 227, 526 G) Sato et al. 1990, ApJ, 359, 192 H) Schutte et al. 1990, ApJ, 360, 577 I) Sellgren 1984, ApJ, 277, 623 J) Tokunaga et al. 1991, ApJ, 380, 452 K) van Citters and Smith 1989, AJ, 98, 1382 L) Whittet et al. 1983, A&A, 123, 301 (see also Blades and Whittet 1980, MNRAS, 191, 701, for HD 97048); M) Whittet et al. 1984, MNRAS, 211, 29 N) This work, Cooled Grating Array Spectrometer (CGAS) A O) This work, CGAS B P) This work, CGS4 Spectrometer --- Note Note flag (a-h) number=3 a) Feature flux from Schutte et al. 1990, ApJ, 360, 577 b) Feature flux from Jourdain de Muizon et al. 1990b, A&A, 227, 526 c) Feature flux from Whittet et al. 1983, A&A, 123, 301 d) Total 3.29 m feature flux estimated from 11.3 m feature (see text). e) Upper limit from Sellgren 1984, ApJ, 277, 623; total feature flux from Sellgren et al. 1985, ApJ, 299, 416 f) Measured flux lower than L(3.45 micron) photometry in Hillenbrand et al. 1992, ApJ, 397, 613, by 35 %. g) Measured flux lower than L(3.45 micron) photometry by 50 %. h) Measured flux higher than L(3.45 micron) photometry by 60 %. --- table2a.tex LaTeX version of table2 (left side) table2b.tex LaTeX version of table2 (right side) Patricia Bauer CDS 1994 Jul 25 AAS CD-ROM series, Volume 1, 1993 UNKNOWN UNKNOWN Other Non-detections: V376 Cas (L), RR Tau (B), VY Mon (E), Z CMa (B), HD 53367 (B), KK Oph (B), V856 Sco (L), MWC 297 (BE), R CrA (DL), T CrA (D), PV Cep (GK). J_AJ_106_656.xml The mass-luminosity relation for stars of mass 1.0 to 0.08 solar masses J/AJ/106/773 J/AJ/106/773 Mass-luminosity relation The mass-luminosity relation for stars of mass 1.0 to 0.08 solar masses T J Henry D W McCarthy Jr. Astron. J. 106 773 1993 1993AJ....106..773H Interferometry Photometry Photometry, infrared Stars, dwarfs Stars, late-type Mass-luminosity relations determined at infrared wavelengths are presented for stars with masses 1.0 to 0.08 solar masses. Using infrared speckle imaging techniques on a sample of nearby binaries, concentration has been on the lower main sequence (Mass<=0.5M_sun_), for which an accurate mass-luminosity calibration has remained problematic. In addition, the mass-visual luminosity relation for stars with 2.0>=Mass>=0.08M_sun_ is produced by implementing new photometric relations linking V to JHK wavelengths for the nearby stars, supplemented with eclipsing binary information. These relations predict that objects with masses ~0.08 solar masses have M(K)~=10 and M(V)~=18.
Basic information and orbital parameters for nearby binaries Gliese Gliese number, from The Catalog of Nearby Stars (Gliese and Jahreiss 1991) --- n_Gliese Note on the star number=1 b: see Mariotti et al. (1990) for mass solution from spectroscopic and speckle data, note that the parallax listed (from Gliese and Jahreiss 1991) will not yield the masses given in Table 5; y: semimajor axis and fractional mass determined via speckle data and photometric relations --- Name Other name --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec plx Parallax arcsec e_plx rms uncertainty on parallax arcsec n_plx Note on plx number=2 a: parallax from Demarque et al. (1986) c: parallax from Harrington (1990) --- P Orbital period yr e_P rms uncertainty on orbital period yr u_P Asterisk, '*' if the error in the period was estimated by the authors --- a Orbital semimajor axis arcsec e_a rms uncertainty on orbital semimajor axis arcsec u_a Asterisk, '*' if the error in the semimajor axis was estimated by the authors --- B Fractional mass of the secondary --- e_B rms uncertainty on B --- n_B Asterisk, '*' if the error in the fractional mass was estimated by the authors --- q_P Orbit quality, numbers from the Fourth Catalog of Orbits of Visual Binary Stars (Worley and Heintz) number=3 Numbers in parentheses are estimates based on their system, "ast" indicates an astrometric binary resolved using infrared speckle techniques, "sp" indicates and orbit derived using infrared speckle and spectroscopic data --- Ref References number=4 References B 55 = Baize 1955, J. Observateurs, 38, 42 E 67 = Eggen 1967, ARA&A, 5, 105 DGV 86 = Demarque et al. 1986, ApJ, 300, 773 GHW 88 = Geyer et al. 1988, AJ, 95, 1841 Ha 90 = Harrington 1990, AJ, 100, 559 Hr 73,82 = Hershey 1973, AJ, 78, 935; 1982, AJ, 87, 145 Hz 69,72,74,76,79,82,86b,87 = Heintz 1969, AJ, 74, 768; 1972, AJ, 77, 160; 1974, AJ, 79, 819; 1976, ApJ, 208, 474; 1979, AJ, 84, 1223; 1982, Observatory, 102, 42; 1986b, A&AS, 65, 411; 1987, PASP, 99, 1084 HzB 84 = Heintz and Borgman 1984, AJ, 89, 1068 HMFC 92 = Henry et al. 1992, AJ, 103, 1369 JHM 93 = Johnson et al. 1993, in preparation KW 78 = Kamper and Wesselink 1978, AJ, 83, 1653 L 82 = Lippincott 1982,, AJ, 87, 1237 LB 78 = Lippincott and Borgman 1978, PASP, 90, 226 LBM 83 = Lippincott et al. 1983, PASP, 95, 271 MHFSLC 88 = McCarthy et al. 1988, ApJ, 33, 943 MH 87 = McCarthy and Henry 1987, ApJ, 319, L93 MHMC 91 = McCarthy et al. 1991, AJ, 101, 214 MM 89 = Marcy and Moore 1989, ApJ, 341, 961 MPDD 90 = Mariotti et al. 1990, A&A, 230, 77 P 77 = Probst 1977, AJ, 82, 656 S 63 = Strand 1963, in Basic Astronomical Data, edited by Harris, Strand and Worley (U. of Chicago Press, Chicago), p.282 V 37 = van den Bos 1937, Union Obs. Circ., 4, 342 V 38 = van den Bos 1938, Union Obs. Circ., 4 448 WH 74 = Worth and Heintz 1974, ApJ, 193, 647 * = this work --- Photometric and infrared speckle photometry Gliese Gliese number, from The Catalog of Nearby Stars (Gliese and Jahreiss 1991) --- lam Wavelength of observation (J, H, K, V) --- m_lam Component observed (A or B) --- n_Phot Note on photometry number=1 r: r for "relations" refers to the fact that in table5, the MV values given have been derived using photometric relations reported section 3.1.1 of the printed paper --- Phot Photometry at the wavelength of observation mag e_Phot rms uncertainty on photometry standard mag r_Phot Reference for the photometry number=2 ESWS = Engels et al. 1981, A&AS, 45, 5 GJ = Gliese and Jahreiss 1991, Preliminary Version of the Third Catalog of Nearby Stars HMFC = Henry et al. 1992, A&A, 254, 116 JMM = Johnson et al. 1968, ApJ, 152, 465 L = Leggett 1992, ApJS, 82, 351 MHMC = McCarthy et al. 1991, AJ, 101, 214 P = Probst 1981 Table A.7, Ph.D. thesis, University of Virginia SH = Stauffer and Hartmann 1986, ApJS, 61, 531 * = this work --- Tech Technique used for observation number=3 1D is one-dimensional infrared speckle imaging, 2D is two-dimensional infrared speckle imaging, NS is north-south scan direction, EW is east-west scan direction, NESW is northeast-southwest scan direction, 1X is an eight-arcsecond field, 2X is a four-arcsecond field --- n_Tech Note on the technique used number=4 'a' for mass determinations, combined 1D observations yield 0.39 arcsec at 44 deg 'b' for mass determinations, combined 1D observations yield 0.90 arcsec to the east 'c' for mass determinations, combined 1D observations yield 1.00 arcsec to the east --- Date UT date "DD/MM/YY" Sepa Separation of binary components arcsec e_Sepa rms uncertainty on separation arcsec PA Position angle of secondary relative to primary deg e_PA rms uncertainty on position angle deg n_PA Note when no value of position angle number=5 a = adopt, N = north, S = sud, E = east, and W = west --- Dm Magnitude difference deg e_Dm rms uncertainty on magnitude difference deg Note Individual notes --- Derived quantities: absolute magnitudes and masses Gliese Gliese number, from The Catalog of Nearby Stars (Gliese and Jahreiss 1991)_ --- M Mass of the object solMass e_M Standard error in mass solMass Vmag Absolute V magnitude for the object mag e_Vmag Absolute V magnitude standard error mag Jmag Absolute J magnitude for the object mag e_Jmag Absolute J magnitude standard error mag Hmag Absolute H magnitude for the object mag e_Hmag Absolute H magnitude standard error mag Kmag Absolute K magnitude for the object mag e_Kmag Absolute K magnitude standard error mag table1.tex TeX version of table1 table2.tex TeX version of table2 table5.tex TeX version of table5 Patricia Bauer CDS 1994 Jul 25 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_773.xml Dynamics of cD clusters of galaxies. I. Redshift data for seven clusters J/AJ/106/831 J/AJ/106/831 cD clusters of galaxies. I. Dynamics of cD clusters of galaxies. I. Redshift data for seven clusters J M Hill W R Oegerle Astron. J. 106 831 1993 1993AJ....106..831H Galaxies, spectra Galaxy catalogs Redshifts The initial results are presented of a spectroscopic study of a sample of cD galaxy clusters. Redshifts are presented for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124.
Velocity data Abell Name of Abell Cluster --- n_Abell '+' when two clusters (399/401) --- ID Cluster identifying number --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Sign of declination --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec cz Observed heliocentric-corrected velocity km/s e_cz rms uncertainty on velocity km/s Com Comments number=1 A letter "E" in the comments field means that the velocity was derived from emission lines only. For galaxy 388 in table4, the listed velocities were derived from emission and absorption lines separately. The letter "A" indicates the presence of absorption lines in the higher Balmer lines. The number of independent measurements contributing to the combined velocity of the cD are also reported. The identifying number of each cD galaxy is 201, except for the A399 cD which is 448 in table4 --- tables.tex LaTeX version of tables Patricia Bauer CDS 1994 Oct 13 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_831.xml On the nature of Mg II absorption line systems in quasars J/AJ/106/848 J/AJ/106/848 QSO MgII absorption line systems On the nature of Mg II absorption line systems in quasars M J Drinkwater R L Webster P A Thomas Astron. J. 106 848 1993 1993AJ....106..848D Galaxies, spectra Photometry, infrared QSOs Redshifts The results of a large R-band imaging survey of 71 bright (m(V)<18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined.
Quasars observed QSO Quasar name --- Type Detection technique number=1 C = color; O = spectral survey; R = radio; X = X-ray --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Vmag Quasar V magnitude mag z Quasar redshift (Data in bytes 1-48 taken from Hewitt & Burbidge 1987, ApJS, 63, 1, and Hewitt & Burbidge 1989, ApJS, 69, 1) --- z1 Minimum redshift at which Mg II might be observed in the published spectra --- z2 Maximum redshift at which Mg II might be observed in the published spectra --- zab1 Redshift of any Mg II absorption systems --- zab2 Redshift of any Mg II absorption systems --- r_z Reference for the published spectra, parentheses signifying a non-detection number=2 References for published spectra |Number| W(rest) | Reference | | 0.1nm ----------------------------------------------------- | 1 | ~ 0.5 | Weyman, et al. 1979, ApJ, 234, 33 | 1a | ~ 0.8 | Weyman, et al. 1979, ApJ, 234, 33 | 2 | 0.6 | Young, et al. 1982, ApJS, 48, 455 | 3 | 0.5 | Foltz, et al. 1986, ApJ, 307, 504 | 4 | | Boulade, et al. 1987, in High Redshift and Primeval | | | Galaxies, edited by J. Bergeron et al. | | (Editions Frontieres, France), p. 349 | 5 | | Miller, et al. 1987, AJ, 94, 633 | 6 | ~ 0.4 | Tytler, et al. 1987, ApJS, 64, 667 | 7 | 0.3 | Sargent, et al. 1988, AJ, 334, 22 | 8 | ~ 0.5 | Bergeron & Boisse 1991, A&A, 243, 344 | 9 | 0.3 | Steidel & Sargent 1992, ApJS, 80, 1 |10 | 0.3 | Bechtold & Ellingson 1992, ApJ, 396, 20 |10a | 0.6 | Bechtold & Ellingson 1992, ApJ, 396, 20 --- Date Date observed (UT) "DD/MM/YY" Epx.T Exposure time s FWHM FWHM seeing arcsec Rmag Quasar R magnitude mag Note Photometry flag number=3 blank: photometric X: not photometric D: double image with magnitude from small DAOPHOT e: no small DAOPHOT fitting was possible --- Rmagl Limiting R magnitude of image (the magnitude of the faintest object for which the formal error in the magnitude was less than 0.2 mag) mag Quasar parameters QSO Quasar name --- z Quasar redshift --- Seeing Seeing arcsec Mlim Magnitude limit mag Catalogue of quasar companions QSO Quasar name --- dRA Right ascension offset from the quasar arcsec dDE Declination offset from the quasar arcsec Dist Distance from the quasar arcsec cls Classification (f: faint, g: galaxy, s: star) --- Rmag Apparent R magnitude, m(R) mag e_Rmag Formal photometry error in the magnitude mag PA Position angle of the object with respect to the quasar, measured anti-clockwise from North deg Patricia Bauer CDS 1994 Sep 07 AAS CD-ROM series, Volume 1, 1993 J_AJ_106_848.xml The dwarf spheroidal companions to M31: a color-magnitude diagram for And III J/AJ/106/986 J/AJ/106/986 CMD for And III The dwarf spheroidal companions to M31: a color-magnitude diagram for And III T E Armandroff G S Da Costa N Caldwell P Seitzer Astron. J. 106 986 1993 1993AJ....106..986A Galaxies, nearby Photometry Photometry, infrared The prime focus CCD camera of the KPNO 4 m telescope has been used to image Andromeda III, a dwarf spheroidal galaxy companion to M31, in the V and I bands.
And III photometry ID Identification number --- x x position pix y y position pix Imag I magnitude mag V-I V-I color mag Marie-Jose Wagner, Patricia Bauer CDS 1994 Oct 25 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_106_986.xml UBVRI Photometry of SN 1993J in M81: The First 120 Days J/AJ/107/1022 J/AJ/107/1022 UBVRI Photometry of SN 1993J in M81 UBVRI Photometry of SN 1993J in M81: The First 120 Days M W Richmond R R Treffers A V Filippenko Y Paik B Leibundgut E Schulman C V Cox Astron. J. 107 1022 1994 1994AJ....107.1022R Photometry, UBVRI Supernovae Photometry of SN 1993J in M81 (NGC 3031) is presented in the Johnson-Cousins UBVRI system, starting within three days of the probable time of explosion and ending 120 days later. The reddening along the line of sight to this supernova is uncertain -- there is evidence for small [E(B-V) ~ 0.08 mag] and moderate [E(B-V) ~ 0.32 mag] values. For each observed flux, the values are corrected for extinction. The colors are fitted to a Planck function, to determine the temperature and total luminosity of the supernova for each value of reddening.
Leuschner 76-cm observations of SN 1993J UT UT date --- JD Julian Date - 2440000 d U U band magnitude The 76 cm telescope's U-band values do not transform well onto the standard color system, but may at least give a qualitative idea of the behavior of SN 1993J at near-UV wavelengths. mag u_U Uncertainty flag for U ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- B B band magnitude mag u_B Uncertainty flag for B ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- V V band magnitude mag u_V Uncertainty flag for V ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- R R band magnitude mag u_R Uncertainty flag for R ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- I I band magnitude mag u_I Uncertainty flag for I ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- Notes C = cloudy, P = poor seeing --- Leuschner 50-cm observations of SN 1993J UT UT date --- JD Julian Date - 2440000 d U U band magnitude mag u_U Uncertainty flag for U ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- B B band magnitude mag u_B Uncertainty flag for B ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- V V band magnitude mag u_V Uncertainty flag for V ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- R R band magnitude mag u_R Uncertainty flag for R ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- I I band magnitude mag u_I Uncertainty flag for I ":" denotes an uncertain value, and "+" one which has been derived using color terms from the previous or following night. --- Notes C = cloudy, P = poor seeing --- La Palma observations of SN 1993J UT UT date --- JD Julian Date - 2440000 d U U band magnitude mag B B band magnitude mag V V band magnitude mag R R band magnitude mag I I band magnitude mag Notes See notes All data are from the 1-m Jacobus Kapteyn Telescope unless marked I. I = Isaac Newton Telescope; P = poor conditions --- Summed optical fluxes of SN 1993J JD Julian Date - 2440000 d Flux Fluxes from measured light curves mW/m2 LowExt Fluxes for extinction [E(B-V)=0.08 mag] mW/m2 ModExt Fluxes for extinction [E(B-V)=0.32 mag] mW/m2 Site Observing site LP = La Palma; KP = Kitt Peak; L = Leuschner --- Bands Bands summed to determine fluxes --- Blackbody temp. and luminosity of SN 1993J JD Julian Date - 2440000 d LowTemp Temp from low ext. [E(B-V)=0.08 mag] K mw/m2 LowLum Bolometric luminosity from LowTemp 10+42 ModTemp Temp from mod. ext. [E(B-V)=0.32 mag] K mW/m2 ModLum Bolometric luminosity from ModTemp 10+42 Site Observing site LP = La Palma; KP = Kitt Peak; L = Leuschner --- Bands Bands used to determine luminosities --- Nancy G. Roman NSSDC/ADC 1994 Oct 25 AAS CD-ROM Vol II J_AJ_107_1022.xml Colors and color gradients in bulges of galaxies J/AJ/107/135 J/AJ/107/135 Colors and color gradients in bulges of galaxies Colors and color gradients in bulges of galaxies M Balcells R F Peletier Astron. J. 107 135 1994 1994AJ....107..135B photometry: galaxies: early-type galaxies: spiral galaxies: photometry We have obtained surface photometry in U, B, R, and I for a complete optically selected sample of 45 early-type spiral galaxies, to investigate the colors and color gradients of spiral bulges. Color profiles in U-R, B-R, U-B, and R-I have been determined in wedges opening on the semiminor axes. Based on several criteria, like the smoothness of the color profiles, the absence of dust lanes, and the central colors, we have defined a subsample of 18 objects whose colors are largely unaffected by dust. We believe such colors are suitable for inferring properties of the stellar populations of bulges. We find that the colors of bulges are predominantly bluer than those of ellipticals. This result holds even when bulges are compared to ellipticals of the same luminosity, and indicates that bulges are younger and/or more metal poor than old elliptical galaxies. Most bulges do not reach solar metallicities. Bulges show predominantly negative color gradients (bluer outward). For bright bulges (M(sup Bulge sub R) is less than -20.0), the magnitude of the gradient increases with bulge luminosity. For fainter bulges, gradients scatter around large negative values. The behavior of color gradients as a function of bulge luminosity suggests different formation mechanisms for faint and bright spheroids. For bright bulges, the scaling of gradients with luminosity suggests a formation process involving dissipation. The similarity with ellipticals suggests that the formation of the disk did not affect the stellar populations of the bulge in a major way. For small bulges (M(sub R) is greater than -20), the existence of pronounced color gradients suggests a different formation mechanism. For these objects, the presence of the disk may have severely affected the radial population distribution in the bulge.
Photometric data UGC UGC denomination --- IC When IC, the following number is the IC name --- NGC NGC denomination --- Type Numerical morphological type from the RC3 --- epsilon Disk ellipticity (1-b/a) --- Mtot(R) R luminosity of the galaxy mag Mbul(R) R luminosity of the bulge mag D/B Bulge to disk ratio in R color --- mu0(R) Central surface brightness of the disk in R color mag/arcsec2 h_UR Ratio of the scale lengths of the disk in U and R minus 1 (h_U/h_R - 1) --- RR Reason why a galaxy did not qualify for the dustfree sample --- Central colors and color gradients NGC NGC name --- (B-R)0 B-R central color mag e_(B-R)0 rms uncertainty on (B-R)0 mag d(B-R)/dr B-R color gradient --- e_d(B-R)/dr rms uncertainty on d(B-R)/dr --- (U-R)0 U-R central color mag e_(U-R)0 rms uncertainty on (U-R)0 mag d(U-R)/dr U-R color gradient --- e_d(U-R)/dr rms uncertainty on d(U-R)/dr --- (R-I)0 R-I central color mag e_(R-I)0 rms uncertainty on (R-I)0 mag d(R-I)/dr R-I color gradient --- e_d(R-I)/dr rms uncertainty on d(R-I)/dr --- (U-B)0 U-B central color mag e_(U-B)0 rms uncertainty on (U-B)0 mag d(U-B)/dr U-B color gradient --- e_d(U-B)/dr rms uncertainty on d(U-B)/dr --- Comparison with aperture photometry NGC Galaxy name --- DeltaU Average difference between the artificial aperture measurement and the literature photometry, in U mag e_DeltaU rms uncertainty on DeltaU mag DeltaB Average difference between the artificial aperture measurement and the literature photometry, in B mag e_DeltaB rms uncertainty on DeltaB mag DeltaR Average difference between the artificial aperture measurement and the literature photometry, in R mag e_DeltaR rms uncertainty on DeltaR mag Integrated colors of single burst models [Fe/H] Metallicity Sun (B-R)20 Integrated B-R color for an age of 20 Gyr mag (B-R)12 Integrated B-R color for an age of 12 Gyr mag Patricia Bauer CDS 1993 Feb 22 J_AJ_107_135.xml Sampling of globular clusters and the distance to the Galactic Center. I. Data description and analysis J/AJ/107/1381 J/AJ/107/1381 Sampling of globular clusters Sampling of globular clusters and the distance to the Galactic Center. I. Data description and analysis C Tello Astron. J. 107 1381 1994 1994AJ....107.1381T Clusters, globular A recent compilation of globular cluster data [Harris, private communication (1991)] has been examined for the purpose of selecting a sufficiently large set of globular clusters with reliable distance estimates. The absolute differences between recent and past estimates of the cluster parameters V(HB) and E(B-V) have been studied in statistically representative (but not mutually exclusive) subsets; resulting in a conservative estimate of the average distance modulus error of 0.40mag for a total selected sample of 134 objects. of spatial and metallicity segregation on the statistics of this sample are investigated. The adopted distance scale uses consistent correction terms for metallicity and reddening according to the precepts in Racine & Harris [AJ, 98, 1609 (1989)].
Derived distance components for 134 selected globular clusters Name Object name number=1 Globular cluster Pal 10 appears in table4.dat although it does not belong to the selected sample S0. --- GLON Galactic longitude deg GLAT Galactic latitude deg V(HB) Estimated level of the horizontal branch mag m/H Metallicity measure [m/H] --- E(B-V) Reddening determination mag Dsun Radial distance from the Sun kpc Xsun X component of distance = Dsun cos b cos l kpc Ysun Y component of distance = Dsun cos b sin l kpc Zsun Z component of distance = Dsun sin b kpc S1 'S1' if S0 cluster revised estimates in V(HB) --- S2 'S2' if S0 cluster revised estimates in E(B-V) --- table4.tex LaTeX version of table4.dat Lee Brotzman ADS 1994, Patricia Bauer [CDS] 21-Oct-1994 Apr 23 Tello C. tello@astmag.lbl.gov Divisao de Astrofisica, Instituto Nacional de Pesquisas Espaciasis (INPE/MCT), CP 515, Sao Jose dos Campos, SP, Brazil AAS CD-ROM series, Volume 2, 1994 J_AJ_107_1381.xml R band polarimetry of Cygnus OB2: Implications for the magnetic field geometry and polarization models J/AJ/107/1433 J/AJ/107/1433 Cygnus OB2 polarimetry R band polarimetry of Cygnus OB2: Implications for the magnetic field geometry and polarization models H A Kobulnicky L A Molnar T J Jones Astron. J. 107 1433 1994 1994AJ....107.1433K Associations, stellar Photometry, infrared Polarization New R band polarimetry is presented of 132 members of the Cygnus OB2 association.
Polarization data GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension J2000.0 h RAm Right ascension J2000.0 min RAs Right ascension J2000.0 s DE- Declination sign --- DEd Declination J2000.0 deg DEm Declination J2000.0 arcmin DEs Declination J2000.0 arcsec Code Coded notes number=1 The coded numbers designate the following: 1) The star appears in Table 7 of Massey & Thompson (1991) and is an association member based on its early type spectra. 2) The star is an early type star based on the UBV photometry by Massey & Thompson (1991); the authors observed 46 such stars tabulated by Molnar & Halas (1994). 3) The star is a member of Cyg OB2 based on UBV photometry by Reddish et al (1966). 4) The star has no published photometry, but is a probable member of the association based on its high polarization. A histogram of stars without photometric measurements reveals they fall into two distinct groups; those with P>2.8% (14 stars) and those with P<1.8% (32 stars). It is improbable that the former are foreground stars, so they are included as likely association members. 5) The star has no published photometry and a low polarization. This does not necessarily preclude membership in Cyg OB2, but makes membership unlikely, and these stars were removed from further analysis in the paper. 6) The star is not a member of Cyg OB2 based on UBV photometry from Massey & Thompson (1991) or Reddish et al (1966) and is not included in any of the analyses in the paper. --- Pol Percent polarization % n_Pol Note for Pol number=2 a) The star has previous photometry results in the literature by either McMillan & Tapia (1977) or Serkowski (1965). b) The star has a close companion, making measurement uncertain. Published photometry and polarimetry should be treated with caution. --- e_Pol rms uncertainty in Pol % PosAng Position angle of polarization deg AV Amount of visual absorption mag RLP Other name in Reddish et al (1966) number=3 Stars numbered "0" indicate no catalog entry for that object. Stars numbered "-1" have multiple catalog entries for the same star. Stars with other negative values are actually a blend of two or more stars and hence the measurements should be regarded as uncertain. --- MT Other name in Massey & Thompson (1991) number=3 Stars numbered "0" indicate no catalog entry for that object. Stars numbered "-1" have multiple catalog entries for the same star. Stars with other negative values are actually a blend of two or more stars and hence the measurements should be regarded as uncertain. --- Sch Other name in Schulte (1956) number=3 Stars numbered "0" indicate no catalog entry for that object. Stars numbered "-1" have multiple catalog entries for the same star. Stars with other negative values are actually a blend of two or more stars and hence the measurements should be regarded as uncertain. --- KMJ Other name in this work number=3 Stars numbered "0" indicate no catalog entry for that object. Stars numbered "-1" have multiple catalog entries for the same star. Stars with other negative values are actually a blend of two or more stars and hence the measurements should be regarded as uncertain. --- table1.tex LaTeX version of table1.dat Lee Brotzman ADS 1994, Patricia Bauer [CDS] 19-Oct-1994 Apr 23 Kobulnicky H.A. chip@ast1.spa.umn.edu Department of Astronomy, University of Minnesota, 116 Church St. SE, Minneapolis, Minnesota 55455 Molnar L.A. lam@astro.physics.uiowa.edu Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa 52242 Jones T.J. tjj@ast1.spa.umn.edu Department of Astronomy, University of Minnesota, 116 Church St. SE, Minneapolis, Minnesota 55455 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_1433.xml Light curves of SN 1993J from the Keck Northeast Astronomy Consortium J/AJ/107/1453 J/AJ/107/1453 Light curves of SN 1993J Light curves of SN 1993J from the Keck Northeast Astronomy Consortium P J Benson W Herbst J J Salzer G Vinton G J Hanson S J Ratcliff P F Winkler D M Elmegreen F Chromey C Strom T J Balonek B G Elmegreen Astron. J. 107 1453 1994 1994AJ....107.1453B Photometry, UBVRI Supernovae BVRI photometry of SN 1993J, and data on its likely progenitor are presented. The post-explosion data were obtained with CCDs attached to telescopes (aperture size 0.4 to 0.6m) on the campuses of the Keck Northeast Astronomy Consortium members by the authors and their students.
KNAC photometry of SN 1993J Obs Observation date (UT) --- JD Julian Date d Bmag B band magnitude mag Vmag V band magnitude mag Rmag R band magnitude mag Imag I band magnitude mag Site Observation site --- table3.tex LaTeX version of table3 Lee Brotzman ADS 1994, Patricia Bauer [CDS] 24-Oct-1994 May 08 Benson P.J. pbenson@lucy.wellesley.edu Whitin Observatory, Wellesley College, Wellesley, Massachusetts 02181 Herbst W., Salzer J.J. and Vinton G. bill@elysium.wesleyan.edu, slaz@parcha.astro.wesleyan.edu Van Vleck Observatory, Wesleyan University, Middletown, Connecticut 06457 Hanson G.J., Ratcliff S.J. ratcliff@midd.cc.middlebury.edu Winkler P.F. winkler@midd.cc.middlebury.edu Middlebury College, Middlebury, Vermont 05753 Elmegreen D.M. elmegreen@vaxsar.vassar.edu Chromey F. chromey@vaxsar.vassar.edu Vassar College, Poughkeepsie, New York 12601 Strom C. and Balonek T.J. tbalonek@center.colgate.edu Foggy Bottom Observatory, Colgate University, Hamilton, New York 13346 Elmegreen B.G. bge@watson.ibm.com IBM Research Division, T. J. Watson Research Center, P.O. Box 218, Yorktown Heights, New York 10598 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_1453.xml The late B-Type Stars: refined MK classification, confrontation with Stromgren photometry, and the effects of rotation J/AJ/107/1556 J/AJ/107/1556 Late B-type stars classification The late B-Type Stars: refined MK classification, confrontation with Stromgren photometry, and the effects of rotation R F Garrison R O Gray Astron. J. 107 1556 1994 1994AJ....107.1556G Spectral types Stars, B-type In the fourth and final of a series of papers on the late B to the early F type stars, the MK spectral classification system for the late B type stars is refined. The effect of rotation on both spectral classification and Stromgren photometry of these stars is considered. The work of Morgan by is extended by the establishment of self-consistent sequences of narrow and broadlined standards. A number of Bp-star classifications are refined and compared with Stromgren photometry.
Spectral types of late B type stars HD HD or DM number --- m_HD multiplicity index --- Name Other identification number=1 Open cluster identification number, Bayer designation, Flamsteed designation, or BSC number, in that order of preference --- b-y b-y color index on the Stromgren system mag m1 m1 index mag c1 c1 index mag Beta Beta index mag Note Indicates a remark in notes file --- Sp Spectral type --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 24-Oct-1994 May 08 Garrison R.F. garrison@centaur.astro.utoronto.ca David Dunlap Observatory, University of Toronto, Box 360, Richmond Hill, Ontario, Canada L4C 4Y6 Gray R.O. grayro@conrad.appstate.edu David Dunlap Observatory, University of Toronto, Box 360, Richmond Hill, Ontario, Canada L4C 4Y6, and Department of Physics and Astronomy, Appalachian State University, Boone, North Carolina 28608 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_1556.xml Reddening estimation for halo red giants using ubvy photometry J/AJ/107/1577 J/AJ/107/1577 Halo red giants reddening Reddening estimation for halo red giants using ubvy photometry B J Anthony-Twarog B A Twarog Astron. J. 107 1577 1994 1994AJ....107.1577A Abundances Magnitudes, absolute Photometry, uvby Stars, giant Stars, metal-deficient Updated uvby observations for a larger sample of metal-deficient red giants are presented and combined with a select sample of data from the literature transformed to a common system. Using the reddening maps of Burstein & Heiles [AJ, 87, 1165 (1982)], new absolute magnitudes, distances, metallicities, and reddenings are derived for each star. The metallicities are determined with a revised calibration of the m1, (b-y) diagram based upon comparison to a compilation of recent spectroscopic abundances transformed to a common system.
uvby photometry of metal-deficient giants ID Identification number=1 Henry Draper, Durchmusterung, or other identification. See explanation of 'Note' field. --- V Visual magnitude mag e_V Standard deviation in V number=2 Errors listed for the magnitude and the indices are standard deviations for a single observation; the standard deviations have been set to 0.000 for stars with only one observation (in field o_b-y or o_c1). It should be emphasized that the probable photometric errors for the stars with V>13.0 and only one observation are significantly larger than implied by the brighter stars. mag b-y b-y color index on the Stromgren system mag e_b-y Standard deviation in b-y number=2 Errors listed for the magnitude and the indices are standard deviations for a single observation; the standard deviations have been set to 0.000 for stars with only one observation (in field o_b-y or o_c1). It should be emphasized that the probable photometric errors for the stars with V>13.0 and only one observation are significantly larger than implied by the brighter stars. mag o_b-y Number of observations for V and b-y number=3 Because the stars were also included in the Caby photometric program (Anthony-Twarog et al. 1991, AJ, 101, 1902), many of the stars have a larger number of V and (b-y) (field N1) than m1 and c1 (field N2). --- m1 m1 index mag e_m1 Standard deviation in m1 number=2 Errors listed for the magnitude and the indices are standard deviations for a single observation; the standard deviations have been set to 0.000 for stars with only one observation (in field o_b-y or o_c1). It should be emphasized that the probable photometric errors for the stars with V>13.0 and only one observation are significantly larger than implied by the brighter stars. mag c1 c1 index mag e_c1 Standard deviation in c1 number=2 Errors listed for the magnitude and the indices are standard deviations for a single observation; the standard deviations have been set to 0.000 for stars with only one observation (in field o_b-y or o_c1). It should be emphasized that the probable photometric errors for the stars with V>13.0 and only one observation are significantly larger than implied by the brighter stars. mag o_c1 Number of observations for m1 and c1 number=3 Because the stars were also included in the Caby photometric program (Anthony-Twarog et al. 1991, AJ, 101, 1902), many of the stars have a larger number of V and (b-y) (field N1) than m1 and c1 (field N2). --- Note Note flag number=4 1 - Identification from Beers et al. 1992, AJ, 103, 1987. 2 - Identification from Beers et al. 1992, AJ, 103, 1987. This star is a brighter giant located near a potential metal-deficient program star; its approximate coordinates are: RA(1950.0) = 23h 24m 00s; DEC(1950.0) = -02d 55m 58s. The actual program star proved to be too faint to produce reliable photometry. --- Derived parameters from table1 ID Identification --- n_E(b-y) Note for derived reddening number=1 An asterisk, '*', indicates that the derived reddening, E(b-y) is from comparisons to the standard c0,(b-y)0 relations, as described in Section 4.3 of the printed paper. --- E(b-y) Reddening mag Mv Absolute magnitude mag R Distance pc l_[Fe/H] Limit flag for [Fe/H] --- [Fe/H] Metallicity Sun [Fe/H]SP Average spectroscopic abundance Sun e_[Fe/H]SP Dispersion in [Fe/H]SP Sun N Number of estimates included in [Fe/H]SP --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 24-Oct-1994 May 08 Anthony-Twarog B.J. and Twarog B.A. anthony@kuphsx.phsx.ukans.edu Department of Physics and Astronomy, University of Kansas, Lawrence, Kansas 66045-2151 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_1577.xml Galaxy structures in the Hercules region J/AJ/107/1629 J/AJ/107/1629 Hercules region galaxies structures Galaxy structures in the Hercules region M Tarenghi B Garilli D Maccagni Astron. J. 107 1629 1994 1994AJ....107.1629T Galaxies Redshifts 216 redshifts have been obtained in a region of 981deg^2^ south of the Hercules supercluster. 172 of these redshifts are of galaxies with mpg<=15.1, 110 of which had no previous velocity measurement. 44 new redshifts are of galaxies fainter than mpg=15.1.
table1 lists all the galaxies with Zwicky magnitude brighter than 15.1 either included in the CGCG (Zwicky et al. 1960; Zwicky & Herzog 1963, 1966) or in the 1990 public version of ZCAT and lying in the area delimited by (RA=14h40m, Dec=-3d), (RA=14h40m, Dec=39d), (RA=16h40m, Dec=39d), (RA=16h40m, Dec=15d), (RA=18h18m, Dec=15d) and (RA=18h18m, Dec=-3d). For the sake of completeness and in order that information can be disseminated, table2 lists all galaxies with either unpublished velocities (44) or morphologies, or for which there is an estimate of the magnitude.
Magnitudes, velocities and morphological classifications of galaxies with mpg <= 15.1 Magnitudes, velocities and morphological classifications of galaxies with mpg > 15.1 RAh Right Ascension 1950.0 h RAm Right Ascension 1950.0 min RAs Right Ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec CGCG Zwicky name --- Name Other name --- l_Vmag limit flag on V --- Vmag Apparent magnitude mag n_Vmag Magnitude note number=1 An asterisk denotes eye estimates for those galaxies not in the CGCG and for the members of double and multiple systems. The eye estimates were obtained by comparison with a certain number (about a dozen) of Zwicky galaxies in the same field on the blue glass copies of the Palomar Observatory Sky Survey (POSS), and they should be within 0.1mag of CGCG measurements. --- Vel Heliocentric velocity km/s n_Vel Velocity note number=2 One of 110 new velocities obtained by M. Tarenghi in the early eighties. --- Type Morphological classification --- n_Type Morphology note number=3 Whenever the morphology was not available in the literature, B. Garilli and D. Maccagni independently classified the galaxies by inspecting the blue glass copies of the POSS. --- Comment General comment about the galaxy --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 24-Oct-1994 May 08 Tarenghi M. mtarengh@eso.org Garilli B. bianca@ifetr.mi.cnr.it Maccagni D. dario@ifetr.mi.cnr.it European Southern Observatory, Garching, Germany AAS CD-ROM series, Volume 2, 1994 J_AJ_107_1629.xml Globular cluster photometry with the Hubble Space Telescope. II. U, V, and I measurements of M15 J/AJ/107/1745 J/AJ/107/1745 HST UVI photometry of M15. II. Globular cluster photometry with the Hubble Space Telescope. II. U, V, and I measurements of M15 B Yanny P Guhathakurta J N Bahcall D P Schneider Astron. J. 107 1745 1994 1994AJ....107.1745Y Clusters, globular Photometry Photometric measurements in V and I of more than 5x10^3^ stars (and in U, V, and I of >~1500 stars) are used to construct color-magnitude diagrams in the central 1' of M15. Fourteen blue straggler candidates are identified in the inner 20".
Stellar photometry and astrometry for M15 (V < 18.1) ID Identification number --- RA Right ascension offset from AC 211=ID 653 number=1 Coordinates are arcsec offsets relative to AC 211 = ID 653. ID 653 is at RA(2000)= 21:29:58.26 DEC(2000)=12:10:02.90 arcsec DE Declination offset from AC 211=ID 653 number=1 Coordinates are arcsec offsets relative to AC 211 = ID 653. ID 653 is at RA(2000)= 21:29:58.26 DEC(2000)=12:10:02.90 arcsec Vmag Visual magnitude mag V-I V-I color mag U-V U-V color mag n_U-V Note for U-V number=2 a - the star is located outside the area covered by the U image. b - the star is not detected in U, though the area was covered. --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 24-Oct-1994 May 17 Yanny B. yanny@guinness.ias.edu Institute for Advanced Study, Princeton, New Jersey 08540 Guhathakurta P. raja@astro.princeton.edu Princeton University Observatory, Peyton Hall, Princeton, New Jersey 08544-1001 Bahcall J.N. jnb@sns.ias.edu Schneider D.P. dps@sns.ias.edu Institute for Advanced Study, Princeton, New Jersey 08540 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_1745.xml RR Lyrae stars and color-magnitude diagram of the globular cluster NGC 6388 J/AJ/107/1764 J/AJ/107/1764 RR Lyrae and CMD of NGC 6388 RR Lyrae stars and color-magnitude diagram of the globular cluster NGC 6388 N A Silbermann H A Smith M Bolte M L Hazen Astron. J. 107 1764 1994 1994AJ....107.1764S Clusters, globular Photometry Photometry is listed in table3 for 407 nonvariable stars in the field which are more than 60 but less than 125 arcsec from the center of NGC 6388, and which have formal uncertainties in each photometric index which are smaller than 0.05 mag. New V, B-V and V, V-R colors are presented for the bulge globular cluster NGC 6388.
Photometry of nonvariable stars in NGC 6388 ID Star number --- X X offset arcsec Y Y offset arcsec Vmag Visual magnitude mag B-V B-V color mag V-R V-R color mag Lee Brotzman ADS 1994, Patricia Bauer [CDS] 24-Oct-1994 May 17 Silbermann N.A. silbermann@msupa.pa.msu.edu Smith H.A. smith@msupa.pa.msu.edu Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824 Bolte M. bolte@lick.ucsc.edu Hubble Fellow, NASA/STScI, UCO and Lick Observatory, University of California, Santa Cruz, California 95064 Hazen M.L. martha@cfa.harvard.edu Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, Massachusetts 02138 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_1764.xml The cyclic period variability in SW Cygni J/AJ/107/1868 J/AJ/107/1868 Cyclic period variability in SW Cyg The cyclic period variability in SW Cygni R C Berrington D S Hall Astron. J. 107 1868 1994 1994AJ....107.1868B Stars, variable Timings of primary eclipse up through 1992 are collected, plus a few overlooked in earlier studies. O-C values are give for each observation.
Times of primary minimum for SW Cygni Cycle Cycle number --- O-C O-C curve value d O-C' O-C' curve value d JD Julian date d Error Uncertainty or error in original source d n_Error Weights assigned by Slovochotova (1954) --- Ref Reference number=1 References: 1. Slovochotova 1954, P.Z., 10, 21 [pg,vp,ve] 2. Whitney 1959, AJ, 64, 258 [pg] 3. Szczepanowska 1956, AcA, 6, 144 [ve] 4. Lange 1959b, Astr. Circ. No. 201, 13 [ve] 5. Lange 1960, Astr. Circ. No. 209, 23 [ve] 6. Walter 1971, A&A, 13, 249 [pe] 7. Hall 1968, IBVS, No. 281 [pe] 8. Hall, Garrison 1972, PASP, 84, 552 [pe] 9. Frieboes-Conde, Herczeg 1973, A&AS, 12, 1 [pe] 10. Hall et al. 1979, AcA, 29, 653 [pe] 11. B.B.S.A.G. [ve] 12. Olson 1981, IBVS Mo. 1938 [pe] 13. Olson 1982, ApJ, 259, 702 [pe] 14. Flin 1983, M.V.S. 9, 89 [ve] 15. Kordylewski 1963, IBVS No. 35 [ve] 16. Scholz 1964, Harthaer Beobachtungs Zirkular No. 28 [pg] 17. B.A.A.V.S.S. [ve] 18. Struve 1946, ApJ, 104, 253 [sp] 19. Baldwin 1973, IBVS No. 795 [ve] 20. Parenago 1931, Russian AJ, 8, 229 [pg,vp] pg = photographic pe = photoelectric sp = spectroscopic ve = visual estimates vp = visual photometer --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 15-Feb-1995 Aug 16 Berrington R.C. & Hall D.S. hallxxds@crtvax.vanderbilt.edu Dyer Observatory, Vanderbilt University, Nashville, Tennessee 37235 AAS CD-ROM series, Volume 3, 1995 J_AJ_107_1868.xml Fabry-Perot measurements of the dynamics of globular cluster cores: M15 (NGC 7078) J/AJ/107/2067 J/AJ/107/2067 Fabry-Perot measurements of M15 Fabry-Perot measurements of the dynamics of globular cluster cores: M15 (NGC 7078) K Gebhardt C Pryor T B Williams J E Hesser Astron. J. 107 2067 1994 1994AJ....107.2067G Clusters, globular Radial velocities Velocities have been measured with uncertainties of less than 5km/s for 216 stars within 1.5' of the center of the globular cluster M15 (NGC 7078) using the Rutgers Imaging Fabry-Perot Spectrometer.
M15 stars ID Star ID, blank indicates continuations number=1 ID is taken from Kuestner, F. 1921, Veroeff. Sternw. Bonn., No. 15, or Auriere, M., & Cordoni, J.P. 1981, A&AS, 46, 347 if the star has been previously studied, or an FP number if it has not. --- Xoff X offset from cluster center number=2 The center of the cluster was taken to be 21h27m33.3s, +11d56m49s (1950), as measured by HST (Lauer, T.R. et al. 1991, ApJ, 369, L45). arcsec Yoff Y offset from cluster center number=2 The center of the cluster was taken to be 21h27m33.3s, +11d56m49s (1950), as measured by HST (Lauer, T.R. et al. 1991, ApJ, 369, L45). arcsec FPVmag Fabry-Perot V magnitude mag RVel Velocity number=3 When there are multiple velocity measurements for the same star, the first line for that star lists the average velocity calculated from all of the measurements weighted by their uncertainties and the following lines are the individual measurements. km/s e_RVel Error in velocity km/s r_RVel Source for velocity number=4 Source of velocity measurement. All the measurements from Peterson R.C., Seitzer P. & Cudworth K.M. 1989, ApJ, 347, 251 (PSC) are included. Other sources are listed as FP91 or FP92 for the authors 1991 or 1992 Fabry-Perot observations. --- ChiSq Chi-square for multiple measurements number=5 Probability of chi-square for multiple measurements being drawn from the same velocity. --- Note Notes number=6 Notes include code numbers, as follows: 1: Binary star candidates 2: Not used in dynamics due to radical FP bias 3: Not used in dynamics due to severe contamination 4: PSC has 33 measurements for this star Other notes include additional ID's for stars, as follows: V: Variable star number (Sawyer-Hogg, H. 1973, Publ. David Dunlap Obs., 3, No. 6) S: Sandage, A. 1970, ApJ, 162, 841 I-V: Roman numerals from Arp, H. C. 1955, AJ, 60, 317 --- table1.tex LaTeX version of Table 1 Lee Brotzman ADS 1994, Patricia Bauer [CDS] 15-Feb-1995 Aug 16 Gebhardt K. gebhardt@physics.rutgers.edu, Pryor C. pryor@physics.rutgers.edu, Williams T.B. williams@physics.rutgers.edu Department of Physics and Astronomy, Rutgers, The State University, Box 0849, Piscataway, New Jersey 08855-0849 Hesser J.E. hesser@dao.nrc.ca Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 W. Saanich Road, R.R.5, Victoria, B.C., V8X 4M6, Canada AAS CD-ROM series, Volume 3, 1995 J_AJ_107_2067.xml Independent Distance Determinations to Milky Way Cepheids in Open Clusters and Associations. I. The Binary Cepheid DL Cas in NGC 129 J/AJ/107/2093 J/AJ/107/2093 DL Cas Independent Distance Determinations to Milky Way Cepheids in Open Clusters and Associations. I. The Binary Cepheid DL Cas in NGC 129 W P Gieren D L Welch J -C Mermilliod J M Matthews G Hertling AJ 107 2093 1994 1994AJ....107.2093G Radial velocities Stars, variable Radial velocities, orbital phases, orbital velocities, orbital O-C's, pulsation phase, and pulsation velocities are given for the eight-day Cepheid, DL Cas, which is both a component of a spectroscopic binary and a member of the open cluster NGC 129.
Radial velocity observations of DL Cas HJD Heliocentric Julian Date - 2400000 day RVel # Radial velocity km/s Instr Instrument, 'DAO' or 'COR' --- OPh Orbital phase --- OVel Orbital velocity km/s O-C Orbital O-C km/s PPh Pulsational phase --- PVel Pulsational velocity km/s Lee Brotzman ADS 1994 Aug 16 J_AJ_107_2093.xml Berkeley 93: a distant star cluster nestled in a dust cloud J/AJ/107/2101 J/AJ/107/2101 Berkeley 93 RVB photometry Berkeley 93: a distant star cluster nestled in a dust cloud W Saurer R Seeberger R Weinberger R Ziener Astron. J. 107 2101 1994 1994AJ....107.2101S Clusters, open Photometry, CCD While performing galactic and extragalactic studies near the galactic plane in Cepheus. CCD frames in B, V, and R were taken of the faint (V>=16m), previously unstudied open star cluster Berkeley 93 (Be 93). Our results indicate that this object is the core of a larger aggregate. is slightly evolved. strongly reddened [E(B-V)~1.5], and shows a pronounced variable reddening that is probably due to the location of the cluster inside (near the border) a dust cloud. By far the reddest, and obviously most evolved star is a (variable) carbon star that-because of its reddening and location-appears to be a cluster member. We present arguments in favor of a large distance of more than 5kpc for Be 93 which possibly belongs to the galactic warp. As an addendum, we present six star concentrations discovered on the POSS or ESO/SERC atlas that might represent hitherto uncatalogued open star clusters of "Berkeley type."
Berkeley 93 C 2154+637 21 56.2 +63 56
Photometry of Berkeley 93 Seq Star sequential number --- Rmag R magnitude mag Vmag V magnitude mag Bmag B magnitude mag V-R V-R colour index mag B-V B-V colour index mag Cl C: cluster star; blank: field star --- James Marcout, Patricia Bauer CDS 1997 Mar 25 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_107_2101.xml A survey of proper motion stars. XII. An expanded sample J/AJ/107/2240 J/AJ/107/2240 Proper motion stars survey. XII. A survey of proper motion stars. XII. An expanded sample B W Carney D W Latham J B Laird L A Aguilar Astron. J. 107 2240 1994 1994AJ....107.2240C Abundances Effective Photometry, UBV Radial velocities Space, velocities New photometry and radial velocities are reported for almost 500 stars from the Lowell Proper Motion Catalog. These results are combined with a prior sample and rederive stellar temperatures based on the photometry, reddening, metallicities (using Chi^2 matching of 22,500 low S/N high resolution echelle spectra with a grid of synthetic spectra), distances, space motions, and Galactic orbital parameters for 1269 (kinematics) and 1261 (metallicity) of the 1464 stars in the complete survey. Four possible new members of the class of field blue stragglers are noted.
Final data for the expanded sample Name Star name number=1 Preference is given to the Giclas designations from the Lowell Proper Motion catalog since the author used their finding charts. A few HD and BD names are used. RA and Dec: the positions were taken directly from the observing catalogs used at the telescopes. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Sign of declination --- DEd Declination (1950) deg DEm Declination (1950) arcmin mu Proper motion arcsec/yr PA Position angle of the proper motion deg RV Mean radial velocity km/s e_RV rms velocity deviation km/s N Number of CfA velocity measurements --- Span Span of the velocity observations d Vmag V magnitude mag B-V B-V color mag U-B U-B color --- GLON Galactic longitude deg GLAT Galactic latitude deg E(B-V) Color excess in B-V --- Teff Effective temperature K e_Teff rms deviation of Teff K M Primary mass solMass l_[m/H] Limit flag on [m/H] --- [m/H] Spectroscopic metallicity Sun d Distance pc U Velocity along a Galactic radius km/s V Velocity tangential to Galactic rotation km/s W Velocity perpendicular to Galactic disk km/s Rap Apo-galacticon distance kpc Rpe Peri-galacticon distance kpc Zm Maximun Z distance perpendicular to Galactic disk kpc Bin Binary status flags number=2 The following note flags apply to the Bin and Comment fields Binary Flags: BC Member of a common proper motion pair BV Visual binary BX Optical (i.e., false) double SO Single-lined system with orbital solution SP Single-lined system with preliminary orbital solution S Single-lined binary system without firm period estimate S? Suspected single-lined binary DO Double-lined system with orbital solution DP Double-lined system with preliminary orbital solution D Double-lined system without firm period estimate D? Suspected double-lined system TO Multiple system with orbital solution TP Multiple system with preliminary orbital solution T Multiple system without firm period estimate T? Suspected multiple system DM Double-lined system suspected from metallicity measures Photometry Flags: EY Eggen's modified UVBY system PY Previously published uvby photometry RY Revised photometry SP Schuster, Parrao, & Contreras Martinez 1993, A&AS, 97, 951 PK Previously published JHK or K photometry NK New JHK or K photometry NV New UBV photometry Special Classes of Stars: TO Probable turn-off star SB Blue straggler candidate SG Subgiant or giant SN Nitrogen-rich dwarf SR Broad-lined spectrum SS Synthetic spectrum standard star ST Good trigonometric parallax target SU Unusually large UV excess SV Photometric variable SX Extreme-velocity star Uncertainties UI Uncertain identification UM Uncertain proper motion UP Uncertain photometry UR Uncertain reddening UV Uncertain radial velocity Extra Notes SF In program of Sandage & Fouts, 1987, AJ, 93, 74 XS In expanded sample -------------------------------------------------------------------------------- Acknowledgements: Carney B.W. bruce@sloth.astro.unc.edu Department of Physics and Astronomy, University of North Carolina, Chapel Hill, North Carolina 27599-3255 Latham D.W. latham@cfa.harvard.edu Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 Lairg J.B. laird@tycho.bgsu.edu Department of Physics and Astronomy, Bowling Green State University, Bowling Green, Ohio 43403 Aguilar L.A. aguilar@bufadora.astrosen.unam.mx Observatorio Astronomico Nacional, Apdo. Postal 877, Ensenada, B.C., Mexico AAS CD-ROM series, Volume 3, 1995 --- Com Comment flags number=2 The following note flags apply to the Bin and Comment fields Binary Flags: BC Member of a common proper motion pair BV Visual binary BX Optical (i.e., false) double SO Single-lined system with orbital solution SP Single-lined system with preliminary orbital solution S Single-lined binary system without firm period estimate S? Suspected single-lined binary DO Double-lined system with orbital solution DP Double-lined system with preliminary orbital solution D Double-lined system without firm period estimate D? Suspected double-lined system TO Multiple system with orbital solution TP Multiple system with preliminary orbital solution T Multiple system without firm period estimate T? Suspected multiple system DM Double-lined system suspected from metallicity measures Photometry Flags: EY Eggen's modified UVBY system PY Previously published uvby photometry RY Revised photometry SP Schuster, Parrao, & Contreras Martinez 1993, A&AS, 97, 951 PK Previously published JHK or K photometry NK New JHK or K photometry NV New UBV photometry Special Classes of Stars: TO Probable turn-off star SB Blue straggler candidate SG Subgiant or giant SN Nitrogen-rich dwarf SR Broad-lined spectrum SS Synthetic spectrum standard star ST Good trigonometric parallax target SU Unusually large UV excess SV Photometric variable SX Extreme-velocity star Uncertainties UI Uncertain identification UM Uncertain proper motion UP Uncertain photometry UR Uncertain reddening UV Uncertain radial velocity Extra Notes SF In program of Sandage & Fouts, 1987, AJ, 93, 74 XS In expanded sample -------------------------------------------------------------------------------- Acknowledgements: Carney B.W. bruce@sloth.astro.unc.edu Department of Physics and Astronomy, University of North Carolina, Chapel Hill, North Carolina 27599-3255 Latham D.W. latham@cfa.harvard.edu Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 Lairg J.B. laird@tycho.bgsu.edu Department of Physics and Astronomy, Bowling Green State University, Bowling Green, Ohio 43403 Aguilar L.A. aguilar@bufadora.astrosen.unam.mx Observatorio Astronomico Nacional, Apdo. Postal 877, Ensenada, B.C., Mexico AAS CD-ROM series, Volume 3, 1995 --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 27 J_AJ_107_2240.xml CCD Photometry of the Globular Cluster NGC 1904 (M79) J/AJ/107/230 J/AJ/107/230 Photometry of NGC 1904 CCD Photometry of the Globular Cluster NGC 1904 (M79) G Alcaino W Liller F Alvarado E Wenderoth Astrophys. J. 107 230 1994 1994AJ....107..230A Clusters, globular Photometry, UBVRI BVRI photometry is presented for three overlapping fields in the globular cluster NGC 1904 (M79), observed with a CCD camera and the 2.2 m Max-Planck-Institute telescope at ESO/La Silla. The file contains coordinates, magnitudes, and colors for 750 stars. Critical comparisons of the photometry using the INVENTORY data reduction code with results derived by other investigators using different codes indicates that all modern codes give results reliable to at least +/- 0.3 mag at all levels, as long as the fields are not overly crowded. Specifically, these results for NGC 1904 (M79) are as follows: V(TO) = 19.60 +/- 0.10 (estimated external error), with turnoff colors at B-V = 0.40, V-R = 0. 27, V-I = 0.57, and B-I = 0.97, all with estimated external errors of +/- 0.06.
Data for 750 stars in NGC 1904 Star Star number Two variables reported by Sawyer-Hogg (1973, Pub. David Dunlop Obs. (University of Toronto Press, Toronto), Vol. 3, No. 6) lie in the observed area, and are marked "V2" (Star 437) and "V4" (Star 470). The 6 standard stars are labelled "B" (Star 311), "C" (Star 714), "D" (Star 385), "E" (Star 303), "F" (Star 289), and "G" (Star 405). Table 4 of the printed paper details the observations of the standards. --- n_Star #Additional note for Star --- X X CCD coordinate pix Y Y CCD coordinate pix V V magnitude mag B-V B-V color mag V-R V-R color mag R-I R-I color mag V-I V-I color mag B-I B-I color mag Nancy G. Roman NSSDC/ADC 1994 Dec 16 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_230.xml Evolved GK stars near the Sun. II. The young disk population. J/AJ/107/594 J/AJ/107/594 Evolved GK stars near the Sun. II. Evolved GK stars near the Sun. II. The young disk population. O J Eggen Astron. J. 107 594 1994 1994AJ....107..594E Space, velocities Stars, giant From a sample of nearly 2000 GK giants a group of young disk stars with well determined space motions has been selected. The zero point of the luminosity calibrations, both from the ultraviolet flux (modified Stromgren system) and that in the region of 4200 to 4900A (DDO system), show a discontinuity of about a half magnitude at the border of the young disk and old disk domains. The population separation is based on the space velocity components, which are also an age discriminants with the population interface near 2x10^9yr, based on models with convective overshoot at the core. This age corresponds to giant masses near 1.7M_{sun}_, near the critical mass separating the young stars that do not burn helium in degenerate cores from older stars that do. Ten percent of both populations show CN anomalies in that the derived value of P[Fe/H] from CN(C_m_) and from Fe(M_1_) differ by more than 0.1dex and the weak and strong CN stars occur equally in the old disk but the weak CN stars predominate in the young disk. Peculiar stars, where flux distortions affect the luminosity calibrations, are of the CH+ (Ba II) and CH- (weak G band) variety and represent less than 1% of the stars in both populations. The young disk giants are restricted to ages greater than about 10^9^yr, because younger stars are bright giants or supergiants (luminosity class II or I), and younger than about 2x10^9yr, because the old disk-young disk boundary occurs near 1.7M_{sun}_. The distribution of heavy element abundances, P[Fe/H], for young disk giants is both more limited in range (+/-0.4dex) and is skewed toward higher abundances, compared with the nearly normal distribution for old disk giants. The distribution of (U,V) velocity vectors gives (U,V,W) and their dispersions =(+17.6+/-18.4, -14.8+/-8.4, -6.9+/-13.0) and (+3.6+/-38.4, -20.7+/-27.5, -6.7+/-17.3) km/s for young and old disk giants, respectively. For a description of the DDO and RI Eggen photometric system, see e.g. <GCPD/12> and <GCPD/17> , respectively.
Photometric indices for giants in galactic clusters Cluster Cluster name --- Star Star designation --- M1 M_1_ index number=1 M1 = m1 (Stroemgren) for (b-y)<0.3mag and C1 (Stroemgren) for (b-y)<0.2mag mag [C1] index mag b-y b-y colour index mag R-I R-I colour index mag E(b-y) Colour excess in b-y number=2 Average values: ---------------------------------------------------------------------- E(b-y) Mod mean P[Fe/H](M1) P[Fe/H](DDO) ---------------------------------------------------------------------- NGC 752 0.023+/-0.07 7.90+/-0.07 -0.21+/-0.03 -0.20+/-0.06 NGC 2423 0.065 0.607 9.32 0.19 +0.08 0.09 IC 4651 0.096 0.018 9.56 0.15 +0.28 0.07 Praesepe 0.000 5.63 0.20 +0.08 0.06 +0.13 0.08 ---------------------------------------------------------------------- mag u_E(b-y) Uncertainty flag on E(b-y) --- V0 V_0_ magnitude mag Cm0 (C_m_)0 index mag D(45-48)0 {DELTA}(45-48)_0_ colour index mag Mv(C1) Absolute V magnitude from C_1_ system mag u_Mv(C1) Uncertainty flag on Mv(C1) --- Mv(DDO) Absolute V magnitude from DDO system mag u_Mv(DDO) Uncertainty flag on Mv(DDO) --- Modm Mean distance modulus number=2 Average values: ---------------------------------------------------------------------- E(b-y) Mod mean P[Fe/H](M1) P[Fe/H](DDO) ---------------------------------------------------------------------- NGC 752 0.023+/-0.07 7.90+/-0.07 -0.21+/-0.03 -0.20+/-0.06 NGC 2423 0.065 0.607 9.32 0.19 +0.08 0.09 IC 4651 0.096 0.018 9.56 0.15 +0.28 0.07 Praesepe 0.000 5.63 0.20 +0.08 0.06 +0.13 0.08 ---------------------------------------------------------------------- mag u_Modm Uncertainty flag on Modm --- P[Fe/H](M1) Metal abundance from M1 system number=2 Average values: ---------------------------------------------------------------------- E(b-y) Mod mean P[Fe/H](M1) P[Fe/H](DDO) ---------------------------------------------------------------------- NGC 752 0.023+/-0.07 7.90+/-0.07 -0.21+/-0.03 -0.20+/-0.06 NGC 2423 0.065 0.607 9.32 0.19 +0.08 0.09 IC 4651 0.096 0.018 9.56 0.15 +0.28 0.07 Praesepe 0.000 5.63 0.20 +0.08 0.06 +0.13 0.08 ---------------------------------------------------------------------- --- u_P[Fe/H](M1) Uncertainty flag on P[Fe/H](M1) --- P[Fe/H](DDO) Metal abundance from DDO system number=2 Average values: ---------------------------------------------------------------------- E(b-y) Mod mean P[Fe/H](M1) P[Fe/H](DDO) ---------------------------------------------------------------------- NGC 752 0.023+/-0.07 7.90+/-0.07 -0.21+/-0.03 -0.20+/-0.06 NGC 2423 0.065 0.607 9.32 0.19 +0.08 0.09 IC 4651 0.096 0.018 9.56 0.15 +0.28 0.07 Praesepe 0.000 5.63 0.20 +0.08 0.06 +0.13 0.08 ---------------------------------------------------------------------- --- u_P[Fe/H](DDO) Uncertainty flag on P[Fe/H](DDO) --- Wide binaries. Name Star name --- E(b-y) Reddening E(b-y) mag (R-I)0 (R-I)0 colour index or {beta} index mag n_(R-I)0 When ), {beta} index in (R-I)0 column --- V0 V_0_ magnitude mag (Cm)0 (C_m_)0 index mag D(45-48)0 {DELTA}(45-48)_0_ colour index mag [C1] index mag (M1)0 (M1)0 or [M1] index mag n_(M1)0 When ), [M1] index in (M1)0 column --- SpType Spectral type --- P[Fe/H](M1) Metal abundance from M1 system --- P[Fe/H](DDO) Metal abundance from DDO system --- Mv([C1]) Absolute V magnitude from C_1_ system mag Mod Distance modulus mag Mv(DDO) Absolute V magnitude from DDO system mag pmRA Proper motion in right ascension mas/yr pmDE Proper motion in declination mas/yr RV Radial velocity km/s Uvel U velocity (away from the galactic center) km/s Vvel V velocity (direction of galactic rotation) km/s Wvel W velocity (toward North Galactic Pole) km/s Young disk population GK giants Additional members of the old disk population Photometric parameters for bright stars not in table 3, based on Geneva photometry HD HD number (Cat. <III/135>) --- E(b-y) Reddening E(b-y) mag (R-I)0 (R-I)0 colour index mag D(45-48)0 {DELTA}(45-48)_0_ colour index mag Mv(DDO) Absolute V magnitude from DDO system mag Mv(C1) Absolute V magnitude from C_1_ system in table3 M_1_ system in table4 [C_1_] system in table 9 mag Cm0 (C_m_)0 index mag P[Fe/H]DDO Metal abundance from DDO system --- P[Fe/H]2 Metal abundance from [M1] system in table3 [C1] system in table4 (M)0 system in table9 --- u_P[Fe/H]2 Uncertainty flag on P[Fe/H][M1] --- V0 V_0_ magnitude mag Mod Distance modulus mag pmRA Proper motion in right ascension mas/yr pmDE Proper motion in declination mas/yr RV Radial velocity km/s u_RV Note on RV number=1 : uncertain; V variable; V? Variable? --- Uvel U velocity (away from the galactic center) km/s u_Uvel Uncertainty flag on Uvel --- Vvel V velocity (direction of galactic rotation) km/s u_Vvel Uncertainty flag on Vvel --- Wvel W velocity (toward North Galactic Pole) km/s u_Wvel Uncertainty flag on Wvel --- SpType Spectral type --- HR HR number (Cat. <V/50>) --- Note Individual notes, x note in Note number=2 Individual notes: Table3: 16467 (m48, 45-48, 42-45)=(6.58, 1.177, 0.856, 0.170)mag from 3 observations. 17459 Possible companion not confirmed by speckle. 17504 Possible spectroscopic binary. 22695 occultation double not confirmed by speckle. 22905 Sp.B., P=91.6d. 27697 Sp.B., P=39.5d. Hyades cluster. 28305/7 Hyades cluster. 30479 R-I is 0.382mag, not 0.392mag as in Eggen (1989PASP..101..366E). 31296 M1=0.527 not 0.463 as printed in Eggen (1984AJ.....89.1606E). 31444 R Eri, not variable. 33146 M1=0.470 not 0.676 as printed in Eggen (1989PASP..101...45E). 33285 In Eggen (1989PASP..101...45E) b-y should be 0.611mag, not 0.605mag, and R-I should be 0.335mag, not 0.344mag. 36217 CK 0ri, variable? 37297 Sp.B., P=189.9d. 37434 Possibly composite. 38751 Equal component binary. 43980 Sp.B., P=111.7d. Companion may affect (M1) 45168 Sp.B., P=428.1d. 47205 Possibly composite. 47973 The companion is apparently optical. A0 V, 13arcsec. (V, b-y, M1, C1, Beta)=(7.53, 0.042, 0.200, 1.007, 2.909)mag 59148 (45-48 , 42-45, 41-42)=(1.226, 0.914, 0.321)mag from 2 observations. Double-lined Sp.B., P=1601 d. DV=0.8mag. The magnitude has been corrected for the companion (Griffin, 1986, Proc. RASC 80, 102). 59878 ADS 6160. (V, B-V)=(8.96, 0.55)mag, F8 V, 11arcsec. The derived modulus would indicate that the companion is a subgiant (see Eggen, 1966RGOB..120..333E). 83240 Sp.B., P=2824d. 87285 M1=0.493 and C1=0.383, misprinted in Eggen (1989PASP..101...45E). 87816 R Vel, not variable. 92214 Sp.B., P=1200d. 95345 Dm= 0.0mag, 0.2arcsec. 140489 45-48=1.196mag, not 1.146 (Eggen, 1990PASP..102..507E). 180262 HD 180243, 86arcsec distant and N/E, is an optical companion. 218670 Sp.B., P=409.6d. Table4: 6595 Magnitude corrected for equal components. 126051 Considered an old disk giant on the basis of W=-61.1km/s. 137126 Sp.B., P=507d. Table9: 82210 DK UMa, V=0.06mag and P=0.92d 125351 Sp.B, P=212d 148856 Sp.B, P=410.6d 196574 Sp.B, P=205.2d --- Young disk stars with wkCN HD HD number (Cat. <III/135>) --- P[Fe/H](Cm) Metal abundance from C_m_ system --- P[Fe/H](M1) Metal abundance from M_1_ system --- Peculiar stars in the young disk population (see Paper I, 1993AJ....106...80E) CHtype CH+ or CH- type --- HD HD number (Cat. <III/135>) --- (R-I)0 (R-I)0 colour index mag D(45-48)0 {DELTA}(45-48)_0_ colour index mag Cm0 (C_m_)0 index mag [C1] index mag Mv(DDO) Absolute V magnitude from DDO system mag Mv([C1]) Absolute V magnitude from C_1_ system mag P[Fe/H](Cm) Metal abundance from Cm system --- P[Fe/H](M1) Metal abundance from M1 system --- HR HR number (Cat. <V/50>) --- SpType Spetral type number=1 From Keenan and McNeil (1989, Cat <III/150>) except for HD 105956, from Houk (1978, Cat. <III/51>) ---- Mod Distance modulus mag Uvel U velocity (away from the galactic center) km/s Vvel V velocity (direction of galactic rotation) km/s Wvel W velocity (toward North Galactic Pole) km/s Bright giants in NGC 2287 Bright giants HD HD number (Cat. <III/135>) --- No Star number in NGC 2287 --- E(b-y) Reddening E(b-y) mag (R-I)0 (R-I)0 colour index mag (M1)0 (M1)0 index mag Cm0 (C_m_)0 index mag (45-48)0 (45-48)_0_ colour index mag (42-45)0 (42-44)_0_ colour index mag D(45-48)0 {DELTA}(45-48)_0_ colour index mag SpType Spectral type number=1 Spectral types from Keenan and McNeil (1989, Cat <III/150>) --- V0 V_0_ magnitude mag [C1] index mag P[Fe/H](DDO) Metal abundance from DDO system number=2 Average values for NGC 2287 P[Fe/H](DDO)=-0.15dex ; P[Fe/H](M1)=-0.07dex ; Mod DDO = 8.87mag --- P[Fe/H](M1) Metal abundance from M1 system number=2 Average values for NGC 2287 P[Fe/H](DDO)=-0.15dex ; P[Fe/H](M1)=-0.07dex ; Mod DDO = 8.87mag --- Mv(DDO) Absolute V magnitude from DDO system mag Mv(C1) Absolute V magnitude from C_1_ system mag u_Mv(C1) Uncertainty flag on Mv(C1) --- Mod Distance modulus from DDO system number=2 Average values for NGC 2287 P[Fe/H](DDO)=-0.15dex ; P[Fe/H](M1)=-0.07dex ; Mod DDO = 8.87mag mag Uvel U velocity (away from the galactic center) km/s Vvel V velocity (direction of galactic rotation) km/s Wvel W velocity (toward North Galactic Pole) km/s Notes Notes --- Values of [Fe/H] (McWilliam 1990ApJS...74.1075M) for stars in table 9 HD HD number (Cat. <III/135>) --- P[Fe/H](Cm) Metal abundance from C_m_ system mag P[Fe/H](M1) Metal abundance from M_1_ system mag [Fe/H] Metallicity Sun Problem stars. HD HD number (Cat. <III/135>) --- E(b-y) Redenning E(b-y) mag (R-I)0 (R-I)0 colour index mag D(45-48)0 {DELTA}(45-48)_0_ colour index mag u_D(45-48)0 Uncertainty flag on D(45-48)0 --- (Cm)0 (C_m_)0 index mag P[Fe/H](DDO) Metal abundance from DDO system --- P[Fe/H](M1) Metal abundance from M1 system --- u_P[Fe/H](M1) Uncertainty flag on P[Fe/H](M1) --- Mv(DDO) Absolute V magnitude from DDO system mag u_Mv(DDO) Uncetrtainty flag on Mv(DDO) --- Mv(C1) Absolute V magnitude from C_1_ system mag u_Mv(C1) Uncetrtainty flag on Mv(C1) --- HR HR number (Cat. <V/50>) --- Apparent motions of stars in table 11 HD HD number (Cat. <III/135>) --- V0 V_0_ magnitude mag Mod Distance modulus mag u_Mod Uncertainty flag on Mod --- pmRA Proper motion in right ascension mas/yr pmDE Proper motion in declination mas/yr RV Radial velocity km/s n_RV V: variable --- Uvel U velocity (away from the galactic center) km/s Vvel v velocity (direction of galactic rotation) km/s Wvel W velocity (toward North Galactic Pole) km/s Sptype Spectral type --- James Marcout, Patricia Bauer CDS 1997 May 26 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_107_594.xml AH Cam: A Metal-Rich RR Lyrae Star with the Shortest Known Blazhko Period J/AJ/107/679 J/AJ/107/679 Short Blazhko Period RR Lyrae Star AH Cam: A Metal-Rich RR Lyrae Star with the Shortest Known Blazhko Period H Smith J Matthews K Lee J Williams N Silbermann M Bolte Astron. J. 107 679 1994 1994AJ....107..679S Photometry, UBV Stars, variable Analysis of 746 new V-band observations of the RR Lyrae star AH Cam obtained during 1989-1992 that AH Cam is a single-mode RR Lyrae star undergoing the Blazhko effect: periodic modulation of the amplitude and shape of its light curve. A low-resolution spectrum of AH Cam indicates that it is relatively metal rich, with Delta S <= 2. The file contains 423 magnitudes as a function of time. Based on the scatter in the comparison-check star data, each observation of AH Cam is accurate to about +/- 0.025 mag.
1989-1990 AH Cam CCD photometry HJD Heliocentric Julian Date of mid exposure - 244000 d d V V magnitude mag Nancy G. Roman NSSDC/ADC 1994 Dec 16 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_679.xml The extreme ultraviolet explorer bright source list J/AJ/107/751 J/AJ/107/751 EUV Explorer bright sources list The extreme ultraviolet explorer bright source list R F Malina H L Marshall B Antia C A Christian C A Dobson D S Finley A Fruscione F R Girouard I Hawkins P Jelinsky J W Lewis J S McDonald K McDonald R J Patterer V W Saba M M Sirk B A Stroozas J V Vallerga P W Vedder A Wiercigroch S Bowyer Astron. J. 107 751 1994 1994AJ....107..751M Space observations Ultraviolet Initial results from the analysis of the Extreme Ultraviolet Explorer (EUVE) all-sky survey (58-740A) and deep survey (67-364A) are presented through the EUVE Bright Source List (BSL). The BSL contains 356 confirmed extreme ultraviolet (EUV) point sources with supporting information, including positions, observed EUV count rates, and the identification of possible optical counterparts. One-hundred twenty-six sources have been detected longward of 200A.
EUVE
The EUVE bright source list Name EUVE name based on J2000 coordinates --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Lex Count rate in Lexan/B filter number=1 Lex, AlC, Dag, Tin, DSL, DSA: Count rate fields are in units of counts/kilosecond. ct/ks n_Lex Note for Lex field number=2 The note flags for the count rate fields are as follows: * Count rate derived from the calibration observation ** Count rate from Patterer et al, 1993, ApJ, 414, L57 --- AlC Count rate in Al/Ti/C filter number=1 Lex, AlC, Dag, Tin, DSL, DSA: Count rate fields are in units of counts/kilosecond. ct/ks n_AlC Note for AlC field number=2 The note flags for the count rate fields are as follows: * Count rate derived from the calibration observation ** Count rate from Patterer et al, 1993, ApJ, 414, L57 --- Dag Count rate in Dagwood filter number=1 Lex, AlC, Dag, Tin, DSL, DSA: Count rate fields are in units of counts/kilosecond. ct/ks n_Dag Note for Dag field number=2 The note flags for the count rate fields are as follows: * Count rate derived from the calibration observation ** Count rate from Patterer et al, 1993, ApJ, 414, L57 --- Tin Count rate in tin filter number=1 Lex, AlC, Dag, Tin, DSL, DSA: Count rate fields are in units of counts/kilosecond. ct/ks n_Tin Note for Tin field number=2 The note flags for the count rate fields are as follows: * Count rate derived from the calibration observation ** Count rate from Patterer et al, 1993, ApJ, 414, L57 --- DSL Count rate, Deep Survey Lexan/B filter number=1 Lex, AlC, Dag, Tin, DSL, DSA: Count rate fields are in units of counts/kilosecond. ct/ks n_DSL Note for DSL field number=2 The note flags for the count rate fields are as follows: * Count rate derived from the calibration observation ** Count rate from Patterer et al, 1993, ApJ, 414, L57 --- DSA Count rate, Deep Survey Al/C filter number=1 Lex, AlC, Dag, Tin, DSL, DSA: Count rate fields are in units of counts/kilosecond. ct/ks n_DSA Note for DSA field number=2 The note flags for the count rate fields are as follows: * Count rate derived from the calibration observation ** Count rate from Patterer et al, 1993, ApJ, 414, L57 --- ID Possible optical counterpart of source --- OtherID Alternate name for possible counterpart --- Type Source or Spectral type of the optical candidate number=3 'CSPN' indicates the central star of a planetary nebula, 'XRB' an X-ray binary system, and 'LMXB' a low mass X-ray binary. --- Vmag Visual magnitude mag ROSAT Name in ROSAT WFC Bright Source Catalog --- Notes General notes or comments number=4 Individual coded notes, separated by commas, as follows: A Source verified using only the skymaps. B Calibration target. C Serendipitous source observed during a calibration pointing. D Private communication from: 1. Marshall H., Carone T. & Fruscione A. 2. Vallerga J. 3. Vedder P. 4. Stringfellow G. E Refer to the following papers: 1. Vennes et al. 1993, ApJ, 410, L119; 2. Marshall, Carone, & Fruscione 1993, ApJ, 414, L53; 3. Patterer et al. 1993, ApJ, 414, L57; 4. Vedder et al. 1993, ApJ, 414, L61; 5. Cully et al. 1993, ApJ, 414, L49; 6. Vallerga, Vedder, & Welsh 1993, ApJ, 414, L65; 7. Warren et al. 1993, ApJ, 414, L69; 8. Finley et al. 1993, ApJ, 417, 259; 9. Stringfellow & Bowyer 1993, in IAU Circular No. 5803, V1974 Cygni. F Three stars, including a white dwarf, are very likely optical counterparts (J. Dupuis, private communication). G DS count rates, accurate to 50%, are provided by J. Vallerga. H A and B stars probably detected as a "UV leak" by EUVE but reported as extreme ultraviolet sources in the ROSAT Bright Source Catalog. I Optical ID confirmed via: 1. High signal-to-noise optical spectra by D. Finley; 2. Photometry or spectroscopy by M. Dopita. J The DS count rate includes the flare occurring during the observation. --- table2.tex The EUVE bright source list (LaTeX version) document.tex Author-supplied table documentation Lee Brotzman ADS 1994, Patricia Bauer [CDS] 21-Oct-1994 Apr 19 Center for EUV Astrophysics, 2150 Kittredge Street, University of California, Berkeley, CA 94720 AAS CD-ROM series, Volume 2, 1994 J_AJ_107_751.xml The metallicities and kinematics of RR Lyrae variables. I. New observations of local stars J/AJ/108/1016 J/AJ/108/1016 Kinematics of local RR lyrae stars. I. The metallicities and kinematics of RR Lyrae variables. I. New observations of local stars A C Layden Astron. J. 108 1016 1994 1994AJ....108.1016L J/AJ/110/2288 : Kinematics of local RR Lyrae. II. (Layden 1995) Abundances, [Fe/H] Photometry Radial velocities Stars, variable In order to study the structure and formation history of the galaxy, we have obtained low-to-moderate dispersion spectra of 302 nearby RR Lyrae variables of Bailey type "ab". We derived abundances, typically accurate to 0.15-0.20dex and calibrated to the Zinn & West (1984ApJS...55...45Z) globular cluster metallicity scale, from the pseudo-equivalent widths of the Ca II K, Hdelta, Hgamma, and Hbeta lines. Radial velocities accurate to between 2 and 30km/s were obtained from the spectra and from the literature. Distances accurate to between 5% and 20% were derived from published apparent magnitudes and Burstein & Heiles (1982AJ.....87.1165B) reddenings. The metallicity distribution of the RR Lyrae stars peaks at [Fe/H]_K_{approx}-1.5, and is narrower than that of the Ryan & Norris (1991AJ....101.1865R) subdwarfs, as expected since the most metal-rich and metal-poor progenitors preferentially appear as stable red and blue horizontal branch stars, rather than as RR Lyrae. The metal-rich tail of the RR Lyrae distribution extends to [Fe/H]_K_{approx}0, and a qualitative analysis of the distribution of distances from the galactic plane shows that the stars in this tail (i.e., [Fe/H]_K_>-1.0) are more concentrated to the plane than the more metal-poor stars. The abundance distribution of the local RR Lyrae stars is in excellent agreement with the changing abundance distributions of distant RR Lyrae stars as a function of galactocentric distance, as derived by Suntzeff et al. (1991ApJ...367..528S), who ascribed this change to systematic variations in horizontal branch morphology (probably age variations) with galactocentric distance. The abundance distribution of the local RR Lyrae stars also agrees well with those of the distant RR Lyrae stars as a function of distance from the galactic plane. There is no evidence for an abundance gradient in this direction, suggesting that gaseous dissipation did not play a major role in the formation of the outer halo.
New data for local RR Lyrae variables Name Variable star name (as in GCVS4, <II/139>) --- [Fe/H] Metal abundance, on Zinn & West (1984ApJS...55...45Z) scale Sun u_[Fe/H] Uncertainty flag on [Fe/H] --- e_[Fe/H] rms uncertainty on [Fe/H] Sun o_[Fe/H] Number of spectra used for [Fe/H] estimate --- <V> Intensity-averaged V magnitude (see n_<V>) mag r_<V> Reference for <V> (see n_<V>) number=1 Intensity-averaged V magnitude reference: a = <V> value from Schmidt 1991AJ....102.1766S b = Layden (1993, Ph.D. dissertation, Yale University) photoelectric photometry c = Layden (1993, Ph.D. dissertation, Yale University) recalibration of photographic photometry d = Photometry from Nikolev et al. 1984, The Mean Light and Colour (B-V and U-B) Curves of 210 Field RR Lyrae Types Stars, (University of Sofia, Sofia) e = GCVS4 <II/139> photometry uncertain --- n_<V> Photometric passband number=2 Photometry passband: V = photoelectric V B = photoelectric B p = photographic v = (photo)visual --- AV Interstellar absorption in V number=3 Interstellar absorption in V, from Burstein & Heiles 1982AJ....187.1165B --- Dist Distance from Sun kpc e_Dist rms uncertainty on distance kpc Z Distance from Galactic plane kpc Rgc Distance from Galactic center, assumes Ro=8kpc kpc RV Systemic radial velocity km/s e_RV Estimated error in measured radial velocity km/s o_RV Number of spectra used in Vrad estimate --- Method Radial velocity combination method number=4 Radial velocity combination method: 1 = fits with standard RV curve 2 = weighted mean 3 = single observation only --- Vsys Final systemic radial velocity number=5 Final systemic radial velocity, a combination of Vrad and values from the literature km/s e_Vsys Estimated error in Vsys km/s u_Vsys ':' indicates disagreement in velocity number=6 A colon, ':', indicates the measured and literature velocity estimates disagree by more than the quoted error; the quoted error may be too small. -------------------------------------------------------------------------------- Acknowledgements: Layden A.C. <alayden@noao.edu> Department of Astronomy, Yale University, P.O. Box 208101 New Haven, Connecticut 06520-8101 AAS CD-ROM series, Volume 3, 1995 --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 31 J_AJ_108_1016.xml The Intrinsic Shape of NGC 3379 J/AJ/108/111 J/AJ/108/111 NGC 3379 The Intrinsic Shape of NGC 3379 T S Statler Astron. J. 108 111 1994 1994AJ....108..111S Galaxies, optical Photometric and kinematic data from the literature are combined with new dynamical models to derive the intrinsic shape of the "standard" elliptical galaxy NGC 3379. The parameters that are best constrained are the dynamical triaxiality T (essentially the triaxiality of the total mass distribution) and the short-to-long axis ratio of the light distribution c_L. The inferred shape is given by a Bayesian probability distribution in the (T,c_L) plane. Assuming a uniform prior, the most probable shape is oblate with a flattening of c_L=.87. The distribution is strongly non-Gaussian, however, and the expectation values, <T>=.31, <c_L>=.75, imply a flatter and more triaxial figure. The 68% highest posterior density region allows more triaxial shapes as long as they are fairly round, or flatter shapes as long as they are nearly oblate. These results are essentially unchanged if the galaxy is assumed to rotate about its short axis, or if it is modeled as an S0 with a negligible-mass disk rather than as an elliptical. The suggestion of Capaccioli et al. [ApJ, 371, 535 (1991)] that NGC 3379 is a rather flat, triaxial S0 galaxy is found to be improbable at the 98% level; this conclusion is largely independent of the bulge-to-disk ratio or the relative rotation speeds of the two components.
NGC 3379 UGC 5902 10 47.8 +12 35
NGC 3379 point estimators, see Sect. 4.3 of the printed paper for full details Index Index to model parameters in tables 1,2,4 --- T Expectation value of dynamical triaxiality --- c_L Exp. value of flattening of light distrib. --- T_p Most probable value of T --- c_Lp Most probable value of c_L --- T_4 Maximum unprojected likelihood, T --- c_L4 Maximum unprojected likelihood, c_L --- phi_E4 Maximum unprojected likelihood, phi_E --- theta_E4 Maximum unprojected likelihood, theta_E --- table5.tex AASTeX version of table5.dat Lee Brotzman ADS 1994 Oct 10 Statler T.S. tss@physics.unc.edu Department of Physics and Astronomy, CB# 3255, University of North Carolina, Chapel Hill, North Carolina 25799-3255 AAS CD-ROM series, Volume 3, 1995 J_AJ_108_111.xml The radio structure of radio loud and radio quiet quasars in the Palomar bright quasar survey. J/AJ/108/1163 J/AJ/108/1163 Radio structure of Quasars The radio structure of radio loud and radio quiet quasars in the Palomar bright quasar survey. K I Kellermann R A Sramek M Schmidt R F Green D B Shaffer Astron. J. 108 1163 1994 1994AJ....108.1163K QSOs Radio sources Images of resolved radio sources in the Palomar Bright Quasar Survey are presented with an angular resolution of 0.5 and 18arcsec. The observed structure of some well resolved radio quiet quasars and AGN's show large scale linear structures or unresolved central cores similar to radio loud objects in the BQS sample as well as the more luminous radio selected quasars. We suggest that at least some of these less luminous radio quiet objects may contain compact central engines characteristic of radio loud quasars and radio galaxies.
Radio data for the bright quasar survey QSO IAU Source designation --- z Redshift --- Bmag B magnitude mag BMag Absolute B magnitude mag S5GHz Total radio flux density at 5GHz in the D configuration mJy l_Ptotal Indicates that Ptotal and R are upper limits; the '<' means "less or equal" --- Ptotal Absolute monochromatic radio luminosity at 5GHz rest wavelength calculated for a spectral index of -0.5 W/Hz R Ratio of radio (5GHz) to optical (4400A) flux density (see also l_Ptotal column) --- RAh Optical right ascension (1950) h RAm Optical right ascension (1950) min RAs Optical right ascension (1950) s RArh Radio right ascension (1950) h RArm Radio right ascension (1950) min RArs Radio right ascension (1950) s DRA Offset in right ascension arcsec DE- Optical declination sign --- DEd Optical declination (1950) deg DEm Optical declination (1950) arcmin DEs Optical declination (1950) arcsec DEr- Radio declination sign --- DErd Radio declination (1950) deg DErm Radio declination (1950) arcmin DErs Radio declination (1950) arcsec DDE Offset in declination arcsec MorphD D-configuration radio morphology number=1 U: Unresolved SR: Slightly resolved Qp: Quasipoint D: Double M: Multiple CD: Core-Double A: Asymmetric --- MorphA A-configuration radio morphology number=1 U: Unresolved SR: Slightly resolved Qp: Quasipoint D: Double M: Multiple CD: Core-Double A: Asymmetric --- Size Overall angular size in arcsec arcsec Size2 Overall angular size in kpc kpc Note Notes detailed in file notes.dat --- Notes of table 1 (27 QSOs concerned) QSO QSO designation --- Text Text of comment (may be on several lines) --- James Marcout, Patricia Bauer CDS 1997 Oct 22 UNKNOWN UNKNOWN Prepared via OCR at CDS. * 22-Oct-1997: Several errors were communicated by H. Andernach <Heinz.Andernach@astro.ugto.mx>; these were corrected. J_AJ_108_1163.xml The OB association LH 58 in the Large Magellanic Cloud J/AJ/108/1256 J/AJ/108/1256 The OB association LH 58 The OB association LH 58 in the Large Magellanic Cloud C D Garmany P Massey J W Parker Astron. J. 108 1256 1994 1994AJ....108.1256G Associations, stellar Photometry, CCD We present CCD photometry and spectroscopy for stars in Lucke-Hodge 58, an isolated OB association in the Large Magellanic Cloud (LMC) northwest of 30 Doradus. The photometric catalog contains 839 stars with UBV magnitudes complete to V~19. We have obtained spectra and classified 35 stars; combined with previous published spectral types, we find 22 O-type stars. The earliest type is O3-4 V, and there are three WR stars in the association. The slope of the initial mass function, Gamma=-1.7+/-0.3, is in good agreement with other LMC associations. The presence of several evolved supergiants with masses about 15-25M_{sun}_ suggests that some star formation took place as early as 10 million years ago, but the majority of stars formed coevally within the past few million years.
UBV photometry of stars in LH 58 ID Star number, in increasing RA order --- Xpos X CCD coordinate pix Ypos Y CCD coordinate pix Vmag V magnitude mag u_Vmag Uncertainty flag for V number=1 A colon, ":", indicates that the error in magnitude or color (i.e. the weighted average of the photometric errors for that star as calculated by DAOPHOT) is greater than two times the error listed in Table 2 in the printed paper. Two colons, "::", indicate errors greater than three times the typical value. -------------------------------------------------------------------------------- Acknowledgements: Garmany C.D. garmany@jila.colorado.edu Joint Institute for Laboratory Astrophysics, Box 440 University of Colorado, Boulder, Colorado 80309-0389 Massey P. massey@noao.edu Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732, Tucson, Arizona 85726-6732 Parker J.W. joel@hrssun.gsfc.nasa.gov Laboratory for Astrophysics and Space Astronomy, Code 681, Goddard Space Flight Center - NASA, Greenbelt, Maryland 20771 AAS CD-ROM series, Volume 3, 1995 --- B-V B-V color mag u_B-V Uncertainty flag for B-V number=1 A colon, ":", indicates that the error in magnitude or color (i.e. the weighted average of the photometric errors for that star as calculated by DAOPHOT) is greater than two times the error listed in Table 2 in the printed paper. Two colons, "::", indicate errors greater than three times the typical value. -------------------------------------------------------------------------------- Acknowledgements: Garmany C.D. garmany@jila.colorado.edu Joint Institute for Laboratory Astrophysics, Box 440 University of Colorado, Boulder, Colorado 80309-0389 Massey P. massey@noao.edu Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732, Tucson, Arizona 85726-6732 Parker J.W. joel@hrssun.gsfc.nasa.gov Laboratory for Astrophysics and Space Astronomy, Code 681, Goddard Space Flight Center - NASA, Greenbelt, Maryland 20771 AAS CD-ROM series, Volume 3, 1995 --- U-B U-B color mag u_U-B Uncertainty flag for U-B number=1 A colon, ":", indicates that the error in magnitude or color (i.e. the weighted average of the photometric errors for that star as calculated by DAOPHOT) is greater than two times the error listed in Table 2 in the printed paper. Two colons, "::", indicate errors greater than three times the typical value. -------------------------------------------------------------------------------- Acknowledgements: Garmany C.D. garmany@jila.colorado.edu Joint Institute for Laboratory Astrophysics, Box 440 University of Colorado, Boulder, Colorado 80309-0389 Massey P. massey@noao.edu Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732, Tucson, Arizona 85726-6732 Parker J.W. joel@hrssun.gsfc.nasa.gov Laboratory for Astrophysics and Space Astronomy, Code 681, Goddard Space Flight Center - NASA, Greenbelt, Maryland 20771 AAS CD-ROM series, Volume 3, 1995 --- table3.tex LaTeX version of table3 Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 31 J_AJ_108_1256.xml Embedded clusters in giant extragalactic HII Regions. I. BVRHalpha photometry J/AJ/108/1276 J/AJ/108/1276 Clusters in GEHRs Embedded clusters in giant extragalactic HII Regions. I. BVRHalpha photometry Y D Mayya Astron. J. 108 1276 1994 1994AJ....108.1276M Equivalent widths H II regions Photometry, H-alpha Photometry in BVR continuum bands and in the emission line of Halpha+ [N II] are presented for a sample of H II complexes in disk, spiral arm and nuclear regions of galaxies NGC 1365, 1566, 2366, 2903, 2997, 3351, 4303, 4449, and 5253. Main sources of errors on H II region photometry are discussed. Errors due to background subtraction are parametrized in terms of background nonuniformity and fractional background contribution and are described separately in the Appendix. Our photometric data are compared with the existing data in the literature. Photometric properties of the sample regions are analyzed statistically and its implications on star formation are briefly discussed. Colors and Halpha+[N II] equivalent widths of nuclear H II regions are found to be distinctly different from disk H II regions, suggesting different star formation histories. We have identified a few high Halpha+[N II] equivalent width regions, which are fainter than average in both emission line and continuum fluxes, thus accounting for the low frequency of occurence of such regions in flux limited samples.
Photometric catalogue of H II regions Gal Galaxies name (g for groups) --- ID H II region numbers number=1 H II region numbers as identified on the charts in the printed paper. --- Xpos X pixel coordinate number=2 X and Y pixel coordinates on the aligned CCD images, which are the same as that appearing on the grid around identification charts. For NGC 4449 the grids contain different pixel numbers than that given in these columns for the reasons mentioned in the text. pix Ypos Y coordinate number=2 X and Y pixel coordinates on the aligned CCD images, which are the same as that appearing on the grid around identification charts. For NGC 4449 the grids contain different pixel numbers than that given in these columns for the reasons mentioned in the text. pix dirRA Direction of RA position number=3 Approximate position of the H II region, along Right Ascension and declination in seconds of arc, with respect to the galactic nucleus. These were obtained by transforming X and Y assuming that the RA-DEC axis is aligned with X-Y axis of the CCD. Since the alignment during observations is only approximate (<=5deg), RA and DEC values away from the center are less accurate, compared to those near the center of the CCD. Thus the positions should be used only for identification purposes. E, W, N, and S preceeding the numbers indicate respectively whether the H II region is to the east, west, north or south of the nucleus of the galaxy. --- posRA Approximate right ascension position number=3 Approximate position of the H II region, along Right Ascension and declination in seconds of arc, with respect to the galactic nucleus. These were obtained by transforming X and Y assuming that the RA-DEC axis is aligned with X-Y axis of the CCD. Since the alignment during observations is only approximate (<=5deg), RA and DEC values away from the center are less accurate, compared to those near the center of the CCD. Thus the positions should be used only for identification purposes. E, W, N, and S preceeding the numbers indicate respectively whether the H II region is to the east, west, north or south of the nucleus of the galaxy. arcsec dirDE Direction of DE position number=3 Approximate position of the H II region, along Right Ascension and declination in seconds of arc, with respect to the galactic nucleus. These were obtained by transforming X and Y assuming that the RA-DEC axis is aligned with X-Y axis of the CCD. Since the alignment during observations is only approximate (<=5deg), RA and DEC values away from the center are less accurate, compared to those near the center of the CCD. Thus the positions should be used only for identification purposes. E, W, N, and S preceeding the numbers indicate respectively whether the H II region is to the east, west, north or south of the nucleus of the galaxy. --- posDE Approximate declination position number=3 Approximate position of the H II region, along Right Ascension and declination in seconds of arc, with respect to the galactic nucleus. These were obtained by transforming X and Y assuming that the RA-DEC axis is aligned with X-Y axis of the CCD. Since the alignment during observations is only approximate (<=5deg), RA and DEC values away from the center are less accurate, compared to those near the center of the CCD. Thus the positions should be used only for identification purposes. E, W, N, and S preceeding the numbers indicate respectively whether the H II region is to the east, west, north or south of the nucleus of the galaxy. arcsec Diam Diam. of aperture for mag. extractions arcsec l_Vmag Limiting character for V --- Vmag V magnitude number=4 V Magnitude, B-V and V-R colors of H II regions after subtracting assumed background. The rms errors on the measured magnitudes are in the range 0.05-0.10, as estimated from measurements on multiple frames. mag B-V B-V color number=4 V Magnitude, B-V and V-R colors of H II regions after subtracting assumed background. The rms errors on the measured magnitudes are in the range 0.05-0.10, as estimated from measurements on multiple frames. mag V-R V-R color number=4 V Magnitude, B-V and V-R colors of H II regions after subtracting assumed background. The rms errors on the measured magnitudes are in the range 0.05-0.10, as estimated from measurements on multiple frames. mag Salpha Log of observed H_alpha+[N II] flux mW/m2 l_W(Ha) Limiting character for W(Ha) --- W(Ha) Emission equivalent width number=5 H_alpha + [N II] emission equivalent width in A with R magnitude as an estimate for the continuum at H_alpha, computed using the equation W(Ha)=1.633E-11*F_alpha/10**(-0.4(R+48.6)) where, F_alpha is the H_alpha + [N II] flux in mW/m^2 (erg/s/cm^2). The measurement errors are <20A. Note that the R band magnitudes used in the above definition include emission from the nebular continuum and lines. 0.1nm Qual Index of photometric quality number=6 An index of photometric quality. It is an integer between 1 and 4 and gives a measure of the background domination for BVR measurements. Higher the index, more sensitive are the colors to the background measurement. See printed paper for details. --- OtherID Id. from other authors when available number=7 Identification from other authors when available. For measurements with bigger apertures, individual GEHRs enclosed within the aperture are indicated. The notations used for identifications are: CM Crillon and Monnet 1969, =1969A&A.....1..449C HK Hodge and Kennicutt 1983, =1983AJ.....88..296H HP Hawley and Phillips 1980, =1980ApJ...235..783H AN Alloin and Nieto 1982, =1982A&AS...50..491A Oka Oka et. al 1974, PASJ, 26, 289 Tpp Prabhu 1980, ApSpSci., 68, 519 L Lindblad, P.O. see Alloin et. al, 1981A&A...101..377A M McCall, Rybski, and Shields 1985, =1985ApJS...57....1M RW Roy and Walsh: 1986MNRAS.223...39R; 1987MNRAS.228..883R; 1988MNRAS.234..977R WR Walsh and Roy: 1989MNRAS.239..297W; 1989ApJ...341..722W -------------------------------------------------------------------------------- Acknowledgements: Mayya Y.D. ydm@tifrvax.tifr.res.in Indian Institute of Astrophysics, Bangalore 560 034, India AAS CD-ROM series, Volume 3, 1995 --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 31 J_AJ_108_1276.xml Hubble Space Telescope photometry of the central regions of Virgo cluster elliptical galaxies. III. Brightness profiles J/AJ/108/1598 J/AJ/108/1598 Virgo cluster ellipticals. III. Hubble Space Telescope photometry of the central regions of Virgo cluster elliptical galaxies. III. Brightness profiles L Ferrarese F C van den Bosch H C Ford W Jaffe R W O'Connell Astron. J. 108 1598 1994 1994AJ....108.1598F Galaxies, photometry Photometry, surface We have used the Planetary Camera on the Hubble Space Telescope to study the morphology and surface brightness parameters of a luminosity- limited sample of fourteen elliptical galaxies in the Virgo cluster. The total apparent blue magnitudes of the galaxies range between 9.4 and 13.4. In this paper, the core brightness profiles are presented, while the overall morphology and the isophotal shapes are discussed in two companion papers [Jaffe et al. AJ, 108, 1567 (1994); van den Bosch et al. AJ, 108, 1579 (1994)]. We show that, in spite of the spherical aberration affecting the HST primary mirror, deconvolution techniques allow recovery of the brightness profile up to 0.2arcsec from the center of the galaxies. We find that none of the galaxies has an isothermal core. On the basis of their morphological and photometrical properties, the galaxies can be divided in two physically distinct groups, referred to as Type I and Type II. All of the Type I galaxies are classified as E1 to E3 in the Revised Shapley Ames Catalog (Sandage & Tammann 1981), while Type II galaxies are classified as E5 to E7. The characteristics of Type II galaxies are explained by the presence of disks component on both the 1 arcsec and the 10 arcsec scales, while Type I galaxies correspond to the classical disk-free ellipticals.
HST
HST surface brightness profile Name Galaxy name --- Dist Distance from center of galaxy arcsec SBa Surface brightness along major axis mag/arcsec2 e_SBa rms uncertainty on SBa mag/arcsec2 SBb Surface brightness along minor axis mag/arcsec2 e_SBb rms uncertainty on SBb mag/arcsec2 Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Nov 08 Ferrarese L. ferrares@jhufos.pha.jhu.edu Ford H.C. ford@jhufos.pha.jhu.edu Johns Hopkins University and Space Telescope Science Institute, Baltimore, Maryland 21218 van den Bosch F.C. vdbosch@strw.leidenuniv.nl Leiden Observatory, Leiden, The Netherlands Jaffe W. jaffe@strw.leidenuniv.nl Leiden Observatory, Leiden, The Netherlands O'Connell R.W. rwo@perseus.astro.virginia.edu University of Virginia, Charlottesville, Virginia 22903 AAS CD-ROM series, Volume 3, 1995 J_AJ_108_1598.xml Globular cluster photometry with the Hubble Space Telescope. III. Blue stragglers and variable stars in the core of M3 J/AJ/108/1786 J/AJ/108/1786 Blue stragglers & variable stars in M3 Globular cluster photometry with the Hubble Space Telescope. III. Blue stragglers and variable stars in the core of M3 P Guhathakurta B Yanny J N Bahcall D P Schneider Astron. J. 108 1786 1994 1994AJ....108.1786G Clusters, globular Photometry Positional data Stars, blue Stars, variable This paper describes Hubble Space Telescope (HST)/Planetary Camera-I images of the core of the dense globular cluster M3 (NGC 5272). Stellar photometry in the F555W (V) and F785LP (I) bands, with a 1 sigma photometric accuracy of about 0.1mag, has been used to construct color-magnitude diagrams of about 4700 stars above the main-sequence turnoff within r<~1' of the cluster center. We have also analyzed archival HST F336W (U) images of M3 obtained by the Wide Field/Planetary Camera-I Instrument Definition Team. The UVI data are used to identify 28 blue straggler (BS) stars within the central 0.29arcmin^2. The specific frequency of BSs in this region of M3, N(BS)/N(V<V(HB)+2)=0.094+/-0.019, is about a factor of 2-3 higher than that found by Bolte et al. [1993, ApJ, 408, L89] in a recent ground-based study of the same region, but comparable to that seen in the sparse outer parts of the same cluster and in HST observations of the core of the higher density cluster 47 Tuc. The BSs in M3 are slightly more centrally concentrated than red giant branch stars while horizontal branch stars are somewhat less concentrated than red giants. The radial distribution of V-selected subgiant and turnoff stars is well fit by a King model with a core radius r(core)=28"+/-2" (90% confidence limits), which corresponds to 1.4pc. Red giant and horizontal branch stars selected in the ultraviolet data (U<18) have a somewhat more compact distribution (r(core)=22.5"). The HST U data consist of 17 exposures acquired over a span of three days. We have used these data to isolate 40 variable stars for which relative astrometry, brightnesses, colors, and light curves are presented. A Kolmogorov-Smirnov test indicates that, typically, the variability for each star is significant at the 95% level. We identify two variable BS candidates (probably of the SX Phe type) out of a sample of ~25 BSs in which variability could have been detected. Most of the variables are RR Lyrae stars on the horizontal branch. All of them have periods P>~8h.
Stellar photometry and astrometry for M3 ID Stellar ID, in order of increasing RA --- RAoff Right ascension (J2000) offset from center number=1 The equinox 2000 coordinate offsets are relative to the star AC 999 (ID #1426): RA_2000 = 13h 42m 11.7s; DE_2000 = +28d 22' 39" arcsec DEoff Declination (J2000) offset from center number=1 The equinox 2000 coordinate offsets are relative to the star AC 999 (ID #1426): RA_2000 = 13h 42m 11.7s; DE_2000 = +28d 22' 39" arcsec Vmag V magnitude, Johnson system number=2 V magnitude and V-I color (Johnson system) magnitude zero points have been adjusted to match ground-based photometry of some brighter stars. mag V-I V-I color number=2 V magnitude and V-I color (Johnson system) magnitude zero points have been adjusted to match ground-based photometry of some brighter stars. mag U-V U-V color mag n_U-V Note on U-V number=3 'a' indicates the star is located outside the area covered by the U image; 'b' indicates the star is not detected in U. --- F555W F555W magnitude (instrumental) number=4 F555W magnitude and F555W-F785LP color (instrumental). The zero points for these magnitudes are approximate and are based on the WF/PC-1 instrument handbook. mag F785LP F555W-F785LP color (instrumental) number=4 F555W magnitude and F555W-F785LP color (instrumental). The zero points for these magnitudes are approximate and are based on the WF/PC-1 instrument handbook. mag X X pixel coordinate pix Y Y pixel coordinate pix CCD PC CCD image on which star appears --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 31 Guhathakurta P. raja@stsci.edu Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218 Yanny B. yanny@guinness.ias.edu Bahcall J.N. jnb@sns.ias.edu Institute for Advanced Study, Princeton, New Jersey 08540 Schneider D.P. dps@astro.psu.edu Institute for Advanced Study, Princeton, New Jersey 08540 and Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, Pennsylvania 16802 AAS CD-ROM series, Volume 3, 1995 J_AJ_108_1786.xml CCD Calibration of the Magnitude Scale for the SSRS2 Sample: The Equatorial Region J/AJ/108/1987 J/AJ/108/1987 The SSRS2 Sample CCD Calibration of the Magnitude Scale for the SSRS2 Sample: The Equatorial Region M V Alonso L N Da Costa D W Latham P S Pellegrini A A E Milone Astron. J. 108 1987 1994 1994AJ....108.1987A Galactic pole, north Galactic pole, south Galaxies, optical Magnitudes Photometry, CCD In this paper we continue our investigation on the isophotal nature, accuracy, and uniformity of the magnitude system adopted in the Southern Sky Redshift Survey extension (SSRS2). Extending our earlier work, we examine galaxies in the equatorial region, primarily in the declination range -17.5 deg <= Dec. <= 0 deg, over a large range of right ascension, covering the southern and northern Galactic caps. For this purpose, we have obtained CCD isophotal magnitudes in the B and R bands for 265 galaxies of different morphological types. Using this larger sample we confirm our earlier claim that the m(SSRS2) magnitudes are very nearly the magnitude measured within the isophote mu_B = 26 mag/arcsec^2, with a dispersion of about 0.30 mag. The relative zero-point offset between our m(SSRS2) magnitudes and CCD photometry is -0.02 mag from all data we have obtained. However, we detect a variation of the zero-point across different regions of the sky of +/- 0.10 mag for regions at large angular separations. We also estimate that the zero-point offset between the m(SSRS2) and Zwicky systems is relatively small (~0.10 mag), which should allow us to combine the data from the SSRS2 and the CfA2 Redshift Survey.
Galaxy sample Galaxy Name of the galaxy --- StScI Space Telescope Science Institute Id. --- RAh Right ascension 1950.0 h RAm R.A. min RAs R.A. s DE- Sign declination --- DEd Declination 1950.0 deg DEm Dec. arcmin DEs Dec. arcsec Type Morph. type, Corwin 1993, private comm. --- mSSRS2 SSRS2 magnitude mag mMCG Morphological Cat. of Galaxies magnitude mag Note Note flags 1 - Galaxies in common with ESO-LV. 2 - Galaxies in common with CGCG. 3 - Surface brightness profiles used in the comparisons with other authors. * - Comments on Individual Galaxies (see notes1.dat) --- Notes to table 1 Note Text of note for object marked with '*' in field 'Note' in table1.dat --- Isophotal magnitudes for observed galaxies Galaxy Name of the galaxy --- Date Observation date --- mB26 CCD magnitude m_B(26) CCD magnitude m_B(26) as measured within (or extrapolated to) the isophote mu_B = 26 mag/arcsec^2 mag e_mB26 Associated error in mB26 mag mR26 CCD magnitude m_R(26) CCD magnitude m_R(26) as extrapolated to the isophote mu_R = 26 mag/arcsec^2 mag e_mR26 Associated error in mR26 mag muBlim Limiting blue isophote, mu_{B,lim} --- muRlim Limiting red isophote, mu_{R,lim} --- table1.tex TeX version of Table 1 and notes table2.tex TeX version of Table 2 useful.tex Macro package required by TeX files CDS 1995 Jul 10 AAS CD-ROM series, Vol. 4, 1995 Lee Brotzman [ADS] 05-May-1995 J_AJ_108_1987.xml VRI Photometry of Globular Clusters in Virgo and Leo Ellipticals J/AJ/108/2087 J/AJ/108/2087 Globular Clusters in Ellipticals VRI Photometry of Globular Clusters in Virgo and Leo Ellipticals E A Ajhar J P Blakeslee J L Tonry Astron. J. 108 2087 1994 1994AJ....108.2087A Clusters, globular Galaxies, optical Photometry Tables 3-12 contain the positions, radial distances, magnitudes, and colors of objects located for each galaxy. Only objects brighter than R=22 and classified by DOPHOT as point sources in the V, R, and I images are included in the tables. The positions are in arcseconds and are relative to the center of the galaxy such that +x is to the west and +y is to the north. The magnitude and colors of each object have been corrected for reddening and absorption according to Equation (1) of the paper and following the values listed in Table 2 of the paper. Please use those values to recover the actual apparent magnitudes of these objects if desired. We present VRI photometry for the globular cluster systems (GCS's) of ten elliptical and S0 galaxies in Virgo and Leo. We find that the V-I color (metallicity) distributions are quite different from galaxy to galaxy. One extreme is represented by NGC 4374 with a narrow, blue distribution. NGC 4472 has a very broad, uniform distribution in color, corresponding to -1.8 < [Fe/H] < +0.47. At the other extreme is NGC 4365, which is weighted towards red colors, and possibly has a peculiar luminosity function. We suggest that this variation of GCS metallicity depends on environment, with formation of high metallicity globular clusters inhibited in higher density environments. We compare color-color plots of the GCS's of these galaxies with the Milky Way GCS and with integrated isochrones. We find good agreement with the galaxies studied here except that the isochrones predict colors which are slightly too bright in the I band for metal-rich clusters. We also consider the radial GC color distributions in these galaxies. We find evidence for a V-I color gradient only in NGC 4374, in the sense of redder clusters toward the center of the galaxy but warn that possible systematic effects must be ruled out with the new data. Lastly, using the surface brightness fluctuation distances to these galaxies, we find supporting evidence for the universality of the globular cluster luminosity function.
NGC 3379 NGC 4365 NGC 4374 NGC 4406 NGC 4458 NGC 4468 NGC 4472 NGC 4489 NGC 4552 NGC 4578 ID Identification number --- Xpos X position relative to center of galaxy arcsec Ypos Y position relative to center of galaxy arcsec Dist Radial distance arcsec Rmag R magnitude mag V-R V-R color mag R-I R-I color mag CDS 1995 Jul 10 AAS CD-ROM series, Vol. 4, 1995 Lee Brotzman [ADS] 24-Apr-1995 J_AJ_108_2087.xml Corrections and additions to the Third Reference Catalogue of Bright Galaxies. J/AJ/108/2128 J/AJ/108/2128 RC3 corrections and additions Corrections and additions to the Third Reference Catalogue of Bright Galaxies. H G Corwin Jr. R J Buta G de Vaucouleurs Astron. J. 108 2128 1994 1994AJ....108.2128C VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991) Galaxy catalogs Lists of corrections and additions to the Third Reference Catalogue of Bright Galaxies (RC3, Cat. <VII/155>) are given. The corrected version of the catalogue (RC3.9b), dated April 1994, is currently available through the national data centers.
Miscellaneous errata in Volumes I and II PGC PGC (Cat. <VII/119>) number --- Unresolved redshift discrepancies. PGC PGC (Cat. <VII/119>) number --- Name Name --- HRV21cm 21 cm RC3 heliocentric radial velocity km/s HRVopt Optical RC3 heliocentric radial velocity km/s HRVNED NED heliocentric radial velocity km/s Com Comments --- Precise positions of double and multiple galaxies Corrected or improved positions of miscellaneous galaxies PGC PGC (Cat. <VII/119>) number --- m_PGC Multiplicity index on PGC --- Name Name --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec u_DEs Uncertainty flag on DEs number=1 For source with declination in degrees and decimal arcminutes, the declination has been transformed in degrees, arcminutes, arcseconds, followed by a colon. --- RA1950h Right ascension (1950) h RA1950m Right ascension (1950) min RA1950s Right ascension (1950) s DE1950- Declination sign --- DE1950d Declination (1950) deg DE1950m Declination (1950) arcmin DE1950s Declination (1950) arcsec u_DE1950s Uncertainty flag on DE1950s number=1 For source with declination in degrees and decimal arcminutes, the declination has been transformed in degrees, arcminutes, arcseconds, followed by a colon. --- Source Source number=2 Sources for positions in Tables 4 and 5: Big : Bigourdan (1919, observations de nebuleuses et d'amas stellaires - Gauthier-Villars, Paris) Bologna: Unpublished, but see Vettolani et al. (1986A&AS...64..247V) BAS : Skiff (1993, priv. comm.) or ESGC (Corwin and Skiff, in prep.) BO : Butcher and Oemler (1985ApJS...57..665B) CE : Corwin and Emerson (1982MNRAS.200..621C) DC : Dressel and Condon (1976ApJS...31..187D) EDC : Clements (1981MNRAS.197..829C) ESO : Lauberts (1982, Cat. <VII/34>) ESO-LV : Lauberts and Valentijn (1989, Cat. <VII/115>) FGH : Freudling, Giovanelli, and Haynes (1988AJ.....96.1791F) Gavazzi: Gavazzi (1987ApJ...320...96G) GH : Gallouet and Heidmann (1971A&AS....3..325G) GHD1 : Gallouet, Heidmann, and Dampierre (1973A&AS...12...89G) GSC : Russell et al (1990, Cat. <I/220>) HC : Corwin (1980MNRAS.191....1C), or unpublished measurements on PSS prints or SERC films w.r.t. SAO or GSC stars. HKA : Hickson, Kindl, and Auman (1989ApJS...70..687H) HKAm : ibid, mean value for entire group IRAS : IRAS Point Source Catalog (1988, Cat. <II/125>) KEBA : Kojoian, Elliott, Bicay, and Arakelian (1981AJ.....86..820K) KEB1 : Kojoian, Elliott, and Bicay (1981AJ.....86..816K) KEB2 : Kajoian, Elliott, and Bicay (1982AJ.....87.1364K) KET1 : Kojoian, Elliott, and Tovmassian (1978AJ.....83.1545K) KET2 : Kojoian, Elliott, and Tovmassian (1981AJ.....86..811K) KOS : Kirshner, Oemler, and Schechter (1978, Cat. <J/AJ/83/1549>) MFG : Marconi, Focardi, and Greggio (1990ApJ...360L..39M) MQ84 : Melnick and Quintana (1984AJ.....89.1288M) RC2 : de Vaucouleurs, de Vaucouleurs, and Corwin (1976, Cat. <VII/112>) RGO : Royal Greenwich Observatory (1911MNRAS..71..509R) SDMA : Spinrad, Djorgovski, Marr, and Aguilar (1985, <J/PASP/97/932>) SDP : Peterson (1973AJ.....78..811P) SGC : Corwin, de Vaucouleurs, and de Vaucouleurs (1985, Cat. <VII/116>) SMBBF : Slezak, Mars, Bijaoui, Balkowski & Fontanelli (1988, Cat. <VII/159>) SMH : Spellman, Madore, and Helou (1989PASP..101..360S) STMW : Schneider, Thuan, Magri, and Wadiak (1990ApJS...72..245S) TM1 : Takase and Miysuchi-Isobe (1984, Cat. <VII/150>) TM2 : Takase and Miyauchi-Isobe (1985, Cat. <VII/150>) TM3 : Takase and Miysuchi-Isobe (1985, Cat. <VII/150>) TM5 : Takase and Miyauchi-Isobe (1986, Cat. <VII/150>) TM6 : Takase and Miyauchi-Isobe (1987, Cat. <VII/150>) TM9 : Takase and Miyauchi-Isobe (1989PNAOJ...1...11T) TS : Thuan and Seitzer (1979ApJ...231..327T) VCC : Bingelli, Sandage, and Tammann (1985AJ.....90.1681B) UGCo : UGC (Nilson, 1973, Cat. <VII/26>) Notes. Distance and position angle from UGC (Nilson 1973, Cat. <VII/26>) galaxies with precise positions, transformed to RA and Dec --- James Marcout, Patricia Bauer CDS 1997 Jun 19 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_108_2128.xml Period-luminosity-metallicity relations, pulsation modes, absolute magnitudes, and distances for population II variable stars J/AJ/108/222 J/AJ/108/222 Pop. II variable stars Period-luminosity-metallicity relations, pulsation modes, absolute magnitudes, and distances for population II variable stars J M Nemec A F Linnell-Nemec T E Lutz Astron. J. 108 222 1994 1994AJ....108..222N Clusters, globular Stars, population II Stars, variable Period-luminosity-metallicity (P-L-[Fe/H]) relations are presented for RR Lyrae stars, Pop. II Cepheids, anomalous Cepheids and SX Phe stars pulsating in the fundamental (F) and first-overtone (H) modes. The relations were derived by fitting regression lines to the observed pulsation periods and mean B, V, and K magnitudes of over 1200 stars in ~40 stellar systems. Analysis of covariance methods, which allow the simultaneous computation of more than one P-L-[Fe/H] relation, were used to estimate the slopes and intercepts. Of the 24 possible P-L-[Fe/H] relations for the four kind of stars, two pulsation modes, and three passbands considered here, 18 relations have been derived -- the others could not be derived because of a lack of photometry in one or more of the three passbands. The slopes for the F and H pulsators were tested for departures from equality for all types of stars and passbands; the results suggest that the observations are consistent with the assumption that, for each kind of star (except possibly the Pop. II Cepheids), the P-L-[Fe/H] relations for the F and H pulsation modes are parallel but vertically offset, with a family of lines corresponding to a range of metallicities. Pulsation modes and absolute magnitudes are presented for the non-RR Lyrae variable stars considered in the analysis, and distances are estimated for the program clusters. It is well established from previous studies that the P-L relations for RR Lyrae stars are approximately flat for the B passband, and have a slope DeltaM(K)/DeltalogP~-2.4 for the K passband. We recover these slopes, and find that the P-L-[Fe/H] relation in V has an intermediate slope, Delta M(V)/DeltalogP=-0.52+/-0.11. A similar dependence of slope on passband is seen for classical Cepheids [see Madore & Freedman, PASP, 103, 933 (1991)]. The available B,V photometry for ~40 of the known globular cluster Cepheids are found to be consistent with Arp's [AJ, 60, 1 (1955)] assumption that Pop. II Cepheids pulsate in the F and H modes (and not in the F mode only, as has often been assumed). The estimated slopes of the corresponding P-L-[Fe/H] relations are Delta M(B)/Delta log P=-1.69+/-0.05 and DeltaM(V)/DeltalogP=-1.93+/-0.05, with a separation between the F and H modes of 0.59 mag in B, and 0.45 mag in V. As in the case of the RR Lyrae stars the redder passband has the steeper slope. We find that 15 of the 21 short-period BL Her Cepheids (P<=8days) appear to be H pulsators, while 15 of the 19 W Cir Cepheids (12<=P<=30days) appear to be F pulsators. The period-amplitude (P-A(B)) diagram suggests that at a given period the first-overtone pulsators have larger amplitudes than the fundamental mode pulsators. For the Anomalous Cepheids the estimated P-L-[Fe/H] relations have slopes DeltaM(B)/DeltalogP=-3.20+/-0.18, and DeltaM(V)/DeltalogP=-3.13+/-0.28. The offsets between the F and H mode relations are 0.68 and 0.66mag in B and V, respectively. The estimated P-L-[Fe/H] relations in B and V for the SX Phe stars have slopes DeltaM(B)/DeltalogP=-2.66+/-0.52 and DeltaM(V)/DeltalogP=-2.56+/-0.54, and the F and H relations are separated by 0.34 and 0.29mag in B and V, respectively. These relations are consistent with the observed period ratio for the double-mode star SX Phe. In a period-amplitude diagram the longest period SX Phe stars have the largest amplitudes, with no dependence on metallicity. The (B-V)0 color range of the SX Phe stars is from 0.12 to 0.29.
Pop. II Cepheids in galactic globular clusters Name Star name --- [Fe/H] Assumed metal abundance --- E(B-V) Assumed reddening --- P Pulsation period d logP Log base 10 of P d Type Type of Cepheid and pulsation mode number=1 Cepheid Types: BL=BL Her WV=W Vir RV=RV Tau Pulsation Modes: F = fundamental mode H = first-overtone mode --- AB Blue amplitude of the Cepheid mag Bmag Assumed mean B magnitude mag B0 Dereddened B magnitude mag Vmag Assumed mean V magnitude mag V0 Dereddened V magnitude mag B-V B-V color mag (B-V)0 Dereddened B-V color mag B0obs Observed M15-normalized apparent B mag number=2 Observed and predicted apparent B and V magnitudes after correcting and normalizing the metallicity and distance to that of M15 (i.e., the magnitudes are the values that the stars would have if they were all at the distance of M15 and had the metallicity [Fe/H] = -2.15). See equation 5 in the printed paper. mag B0pred Predicted M15-normalized apparent B mag number=2 Observed and predicted apparent B and V magnitudes after correcting and normalizing the metallicity and distance to that of M15 (i.e., the magnitudes are the values that the stars would have if they were all at the distance of M15 and had the metallicity [Fe/H] = -2.15). See equation 5 in the printed paper. mag V0obs Observed M15-normalized apparent V mag number=2 Observed and predicted apparent B and V magnitudes after correcting and normalizing the metallicity and distance to that of M15 (i.e., the magnitudes are the values that the stars would have if they were all at the distance of M15 and had the metallicity [Fe/H] = -2.15). See equation 5 in the printed paper. mag V0pred Predicted M15-normalized apparent V mag number=2 Observed and predicted apparent B and V magnitudes after correcting and normalizing the metallicity and distance to that of M15 (i.e., the magnitudes are the values that the stars would have if they were all at the distance of M15 and had the metallicity [Fe/H] = -2.15). See equation 5 in the printed paper. mag MBobs Observed absolute B magnitude mag MBpred Predicted absolute B magnitude mag MVobs Observed absolute V magnitude mag MVpred Predicted absolute V magnitude mag Ref Reference for source of data number=3 References: C88 = Clement, Sawyer Hogg & Yee 1988, AJ, 96, 1642 CS78 = Clement & Sawyer Hogg 1978, AJ, 83, 167 D69 = Demers 1969, AJ, 74, 926 DH74 = Demers & Harris 1974, AJ, 79, 627 DC67 = Dickens & Carey 1967, Roy. Obs. Bull. no. 129, p. E335 E72 = Eggen 1972, ApJ, 172, 639 G93 = Gonzalez 1993, Ph.D. thesis, U. of Washington, Seattle, WA H85 = Harris 1985, in Cepheids: Theory and Observations. IAU Colloquim No. 82, edited by B. F. Madore (Cambridge University Press, Cambridge), p. 232 K68 = Kwee 1968, Bulletin Astron. Inst. Netherlands, 19, 374 L74 = Lee 1974, Observatory, 94, 74 PM77 = Pike & Meston 1977, MNRAS, 180, 613 PR77 = Pinto & Rosino 1977, A&AS, 28, 427 W86 = Wehlau et al. 1986, AJ, 91, 1340 WS84 = Wehlau & Sawyer Hogg 1984, AJ, 89, 1005 WS85 = Wehlau & Sawyer Hogg 1985, AJ, 90, 2514 W92 = Wehlau 1992, private communication --- Anomalous Cepheids: puls. modes and abs. mags Name Star name --- [Fe/H] Assumed metal abundance --- E(B-V) Assumed reddening --- Ph Pulsation period h Pd Pulsation period d logP Log base 10 of P d Mode Pulsation mode number=1 Pulsation Modes: F = fundamental mode H = first-overtone mode --- Bmag Assumed mean B magnitude mag B0 Dereddened B magnitude mag AB B pulsation amplitude mag Vmag Assumed mean V magnitude mag V0 Dereddened V magnitude mag AV V pulsation amplitude mag B-V B-V color mag (B-V)0 Dereddened B-V color mag B0obs Observed M15-normalized apparent B mag mag B0pred Predicted M15-normalized apparent B mag mag dB0 Difference between B0obs-B0pred mag V0obs Observed M15-normalized apparent V mag mag V0pred Predicted M15-normalized apparent V mag mag dV0 Difference between V0obs-V0pred mag MBobs Observed absolute B magnitude mag MBpred Predicted absolute B magnitude mag MVobs Observed absolute V magnitude mag MVpred Predicted absolute V magnitude mag SX Phe Stars: pulsation modes and abs. mags Name Star name --- [Fe/H] Assumed metal abundance --- r_[Fe/H] Source of metal abundance number=1 References for [Fe/H] ADZ = Armandroff, Demarque & Zinn 1993, BM = Burki & Meylan 1986, A&A, 159, 261 EI = Eggen & Iben 1989, AJ, 97, 431 GMC = Geisler, Minniti & Claria 1992, AJ, 104, 627 KK = Kaluzny & Krzeminski 1993, MNRAS, 264, 785 MB = McNamara & Budge 1985, PASP, 97, 322 MF = McNamara & Feltz 1980, PASP, 90, 275 ZW = Zinn & West 1984, ApJS, 55, 45 --- E(B-V) Assumed reddening --- r_E(B-V) Source of reddening number=2 References for B-V FRN = Fahlman, Richer & Nemec 1991, ApJ, 380, 124 RF = Richer & Fahlman 1988, ApJ, 325, 218 Z85 = Zinn 1985a, ApJ, 293, 424 --- Pm Pulsation period min Pd Pulsation period d logP Log base 10 of P --- Mode Pulsation mode number=3 Pulsation Modes: F = fundamental mode H = first-overtone mode --- B Assumed mean B magnitude mag B0 Dereddened B magnitude mag V Assumed mean V magnitude mag V0 Dereddened V magnitude mag AV V pulsation amplitude mag B-V B-V color mag (B-V)0 Dereddened B-V color mag B0obs Observed M15-normalized apparent B mag mag B0pred Predicted M15-normalized apparent B mag mag dB0 Difference between B0obs-B0pred mag V0obs Observed M15-normalized apparent V mag mag V0pred Predicted M15-normalized apparent V mag mag dB0 Difference between V0obs-V0pred mag MBobs Observed absolute B magnitude mag MBpred Predicted absolute B magnitude mag MVobs Observed absolute V magnitude mag MVpred Predicted absolute V magnitude mag table4.tex TeX version of table4.dat table5.tex TeX version of table5.dat table6.tex TeX version of table6.dat Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 10 Nemec J.M. nemec@das.nrc.ca Department of Astronomy, University of Washington, Seattle, Washington 98195 and Program in Astronomy, Washington State University, Pullman, Washington 99164 Linnell Nemec A.F. anemec@galaxy.gov.bc.ca International Statistics & Research Corporation, Brentwood Bay, British Columbia, Canada V8M 1R3 Lutz T.E. tlutz@beta.math.wsu.edu Program in Astronomy, Washington State University, Pullman, Washington 99164 AAS CD-ROM series, Volume 3, 1995 J_AJ_108_222.xml Photographic astrometry of binary and proper-motion stars. VIII. J/AJ/108/2338 J/AJ/108/2338 Photographic astrometry. VIII. Photographic astrometry of binary and proper-motion stars. VIII. W D Heintz Astron. J. 108 2338 1994 1994AJ....108.2338H I/237 : The Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996) V/39 : 4th Catalog of Orbits of Visual Binaries (Worley+, 1983) J/ApJS/74/275 : Observations of double stars. XIV. (Heintz 1990) J/ApJS/83/351 : Observations of double stars. XV. (Heintz, 1992) J/ApJS/99/693 : Observations of double stars. XVI. (Heintz 1995) J/ApJS/105/475 : Observations of double stars. XVII. (Heintz 1996) Heintz & Borgman, Paper I. 1984AJ.....89.1068H Heintz, Paper II. 1986AJ.....92..446H Heintz, Paper III. 1987AJ.....94.1077H Heintz, Paper IV. 1988AJ.....96.1072H Heintz, Paper V. 1990AJ.....99..420H Heintz, Paper VI. 1991AJ....101.1071H Heintz, Paper VII. 1993AJ....105.1188H Parallaxes, trigonometric Proper motions Stars, double and multiple Stars, masses 300 trigonometric parallaxes, 15 revised binary-star orbits, and 24 mass ratios are listed and annotated.
Proper motions and parallaxes RAh Right ascension (1900) h RAdm Right ascension (1900) (deci-minutes) 0.1min RA2000dm Right ascension (2000) (deci-minutes) 0.1min DE- Declination sign (1900) --- DEd Declination (1900) deg DEm Declination (1900) arcmin DE2000- Declination sign (2000) --- DE2000m Declination (2000) arcmin Note Note number=1 c: combined C: combined with pair BC (1987) m: mean w: with orbit i: BD+2 348 : including 1970 result BD+68 278 A: including 1966 result BD+19 872 : including 1986 result BD+29 1664 : including 1979 result BD+12 1944 : including 1979 result BD+40 2903 : including 1971 result BD+31 3767 : including 1968 result BD-5 5715 : including all earlier meas. BD+29 4741 : including 1951 result BD+15 4733 : including 1982 result r: BD+56 1459 : revised 1981 result --- Name Name --- Names Other name --- Vmag Visual magnitude mag n_Vmag v for variable, + unexplained --- SpType Spectral type --- pmRA Proper motion in right ascension mas/yr pmDE Proper motion in declination mas/yr n_pmRA Note on proper motions number=2 Terms: f: orbital q: time-quadratic a: (cg ABCc) for zeta CnC Cc b: cg for ksi UMa A --- plxr Relative parallax mas u_plxr Uncertainty flag on plxr --- e_plxr rms uncertainty on plxr mas plxabs Absolute parallax arcsec N Number of observations (night means) used --- Int1 Time interval (first year) --- --- Dash --- Int2 Time interval (last year) --- mDisk Magnitude reduction of target star(s) by rotating disks mag n_mDisk v: variable --- mf Average magnitude of the reference-star frame mag n_mf Unexplained symbol --- Me Measurer number=3 The Grant machine was used except for six binaries (*) processes at the Ridell machine --- Revised orbits RAh Right ascension (2000) h RAdm Right ascension (2000), deci-minutes 0.1min DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin Name ADS/Name --- mA Magnitude of the primary mag mB Magnitude of the secondary mag SpType Spectral type --- P Period yr n Yearly motion deg/yr T Time of perihelion passage yr a Semi-major axis arcsec e Eccentricity --- i Inclination angle deg w Longitude of perihelion deg W2000 Longitude of ascending node, 2000 deg n_W2000 Unexplained flag --- Com Comments --- Mass ratios Name ADS/Name --- dm Brightness difference mag e_dm rms uncertainty on dm mag beta Fractional luminosity of the secondary --- e_beta rms uncertainty on beta --- n_beta s: separated --- f-beta Measured motion f-{beta} of the center of light --- e_f-beta rms uncertainty on f-beta --- f Fractional mass (B/(A+B)) --- e_f rms uncertainty on f --- Notes Name Star name --- Name2 Name of the second star when pair --- Ntot Total number of line for the note reference --- Nline Running line number in range [1,Ntot] --- Note Text of the note --- James Marcout, Patricia Bauer CDS 1998 May 05 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_108_2338.xml Emission-line candidates from the northern HK survey J/AJ/108/268 J/AJ/108/268 HK survey emission-line candidates positions Emission-line candidates from the northern HK survey T C Beers W Bestman R Wilhelm Astron. J. 108 268 1994 1994AJ....108..268B J/ApJS/76/1001 : UBV photometry of HK survey stars (Preston+, 1991) J/PASP/102/1392 : UBV photometry from HK survey. I (Doinidis+ 1990) J/PASP/103/973 : Photoelectric UBV from HK survey. II (Doidinis+ 1991) J/AJ/112/1188 : HK survey emission-line candidates (Beers+ 1996) Stars, emission This paper presents a list of 158 candidate emission-line objects detected with the northern HK interference-filter/objective-prism survey obtained with the Burrell Schmidt telescope. The objects have magnitudes in the range 11=<B=<15.5, several magnitudes fainter than obtained with prism surveys of similar resolution. (The HK filter restricts the passband to the region around the H and K lines of Ca II)
Emission-line candidates Plate Burrel Schmidt plate number --- Star Star number --- m_Star An asterisk denotes candidates which were previously discovered and listed in table2 --- BC Brightness classification number=1 vb: very bright b: bright mb: medium bright m: medium mf: medium faint f: faint vf: very faint --- RAh Right ascension 2000 h RAm Right ascension 2000 min RAs Right ascension 2000 s DE- Declination sign --- DEd Declination 2000 deg DEm Declination 2000 arcmin DEs Declination 2000 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Com Comments --- Previous identifications and classifications Plate Burrel Schmidt plate number --- Star Star number --- RAh Right ascension 2000 h RAm Right ascension 2000 min RAs Right ascension 2000 s DE- Declination sign --- DEd Declination 2000 deg DEm Declination 2000 arcmin DEs Declination 2000 arcsec Names Other names --- Sp Spectral classification --- Notes Notes or references number=1 S86c (Stephenson C.B., 1986AJ.....92..139S) S86b (Stephenson C.B., 1986AJ.....91..144S) NLTT NLTT catalogues (Catalogue <I/98>) --- James Marcout, Patricia Bauer CDS 1996 May 28 UNKNOWN UNKNOWN Scanned and processed via OCR at CDS. J_AJ_108_268.xml The Montreal Blue Galaxy Survey. II. Second list of UV-bright candidates J/AJ/108/405 J/AJ/108/405 Montreal Blue Galaxy Survey. II. The Montreal Blue Galaxy Survey. II. Second list of UV-bright candidates R Coziol S Demers M Pena R Barneoud Astron. J. 108 405 1994 1994AJ....108..405C J/AJ/105/35 : Montreal Blue Galaxy Survey (I) (Coziol+ 1993) Galaxies, UV-excess We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B<15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.
Second list of UV-bright galaxies Name Name of the object --- RAh Right ascension, 1950 h RAm Right ascension, 1950 min RAs Right ascension, 1950 s DE- Sign of Declination, 1950 --- DEd Declination, 1950 deg DEm Declination, 1950 arcmin DEs Declination, 1950 arcsec Bmag APM B magnitude mag n_Bmag '*' means B taken from NED --- U-B APM (U-B) color mag IRAS IRAS source, 'yes' or 'no ' --- MB Absolute B magnitude mag XID Cross ID from NASA Extragalactic DB (NED) --- Note Spectrum or note available number=1 An 's' means one spectrum was taken; 'n' signifies a note found in NED for this object and is in the Appendix to the printed paper. --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 10 Coziol R. coziol@astro.umontreal.ca Demers S. demers@astro.umontreal.ca Barneoud R. barneoud@astro.umontreal.ca Departement de Physique, Observatoire du Mont Megantic, Universite de Montreal, Montreal, Quebec, H3C 3J7 Canada Pena M. miriam@astroscu.unam.mx Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Apdo. Postal 70-264, 04510 Mexico D.F., Mexico AAS CD-ROM series, Volume 3, 1995 J_AJ_108_405.xml The space density and kinematics of blue metal-poor main sequence stars near the solar circle J/AJ/108/538 J/AJ/108/538 Metal-poor MS stars UBV photometry The space density and kinematics of blue metal-poor main sequence stars near the solar circle G W Preston T C Beers S A Shectman Astron. J. 108 538 1994 1994AJ....108..538P J/AJ/103/267 : Spectrocopy of hot stars in galactic halo (Beers+ 1992) J/AJ/103/1987 : Stars of very low metal abundance (Beers+ 1992) J/ApJS/76/1001 : UBV photometry of HK survey stars (Preston+, 1991) Photometry, UBV Radial velocities Stars, blue Stars, metal-deficient From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15<(B-V)_0_<0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S_BMP_~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S_BMP_=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}_r.phi.tetha_~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15<(B-V)0<0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.
BMP stars identified photometrically in the HK survey Field HK survey field number --- Star Star number in the filed --- GLON Galactic longitude deg GLAT Galactic latitude deg E(B-V) (B-V) colour excess adopted estimate mag V0 Reddening-corrected apparent V magnitude mag (B-V)0 Reddening-corrected B-V colour index mag (U-B)0 Reddening-corrected U-B colour index mag D0 Color parameter number=1 D0 is the perpendicular distance of each star from the linearized two-color main sequence relation for [Fe/H]=0.0 in the (U-B)_0_ vs (B-V)_0_ plane. --- HRV Heliocentric radial velocity km/s r_HRV Reference for heliocentric radial velocity number=2 Sources. 1. Beers et al., 1992, Cat. <J/AJ/103/267> 2. Beers et al., 1992, Cat. <J/AJ/103/1987> 3. Preston et al., 1991, Cat <J/ApJS/76/1001> 4. This paper --- r_UBV Reference for UBV data number=1 D0 is the perpendicular distance of each star from the linearized two-color main sequence relation for [Fe/H]=0.0 in the (U-B)_0_ vs (B-V)_0_ plane. --- New UBV observations of HK survey stars Repeat UBV observations of HK survey stars Field HK survey field number --- Star Star number in the field --- Vmag mag V magnitude mag B-V B-V colour index mag U-B colour index mag James Marcout, Patricia Bauer CDS 1997 Mar 21 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_108_538.xml BVI CCD photometry of galactic globular clusters. II. M 68 J/AJ/108/555 J/AJ/108/555 M68 galactic globular clusters photometry BVI CCD photometry of galactic globular clusters. II. M 68 A R Walker Astron. J. 108 555 1994 1994AJ....108..555W Clusters, globular Colors Photometry A total of 363 CCD frames in the B, V, and I passbands have been used to study the color-magnitude diagram (CMD) and the variable-star population of the metal-poor galactic globular cluster M68 (NGC 4590, C1236-264). Light curves have been prepared for 40 RR Lyrae variables, five of which are new discoveries, and for two probable SX Phe stars. The RR Lyraes have <V>=15.64+/-0.01, and via several methods E(B-V)=0.07+/-0.01. [Fe/H]=-2.1 is adopted. From a comparison with Sandage's data for M3 (NGC 5272, C1339+286), a period shift of Delta(logP)/Delta([Fe/H])=-0.11+/-0.02 is derived, and the mass-to-light parameter is found to be <A>=1.90. RR Lyrae masses are derived from Fourier fits to the light curves, from the RRd variables, and by comparison with HB (horizontal branch) evolutionary models calculated by Dorman. The light-curve structure agrees qualitatively with recent theoretical models. From short exposures, CMDs have been prepared that are complete from the tip of the red giant branch (RGB) to below the level of the HB, while from the long exposures a CMD to V~23 is provided for 7298 stars more than 158 arcsec distant from the cluster center. The HB is skewed to the blue with the eight bluest stars clearly separated from the remainder of the HB stars. This HB gap is at the identical color to that in M15 (NGC 7078, C2127+119), but M68 lacks the extensive population of the very blue HB stars present in M15. The total number of HB stars is deficient with respect to the RGB population, with the ratio of RGB to HB stars R=0.99. There are several likely blue stragglers identified on CMDs of inner annuli, but near to the cluster center photometric errors scatter stars off the main sequence (MS) into this region. The deep CMDs are in excellent agreement with existing CCD CMDs for M68, with the MS turnoff Delta(V)=3.42+/-0.10mag below the HB. Matching the M68 CMD to that for M15 in the subgiant-MS turnoff region shows that the age of M68 is identical to that for M15 to within +/-0.4Gyr.
Photometry of the RR Lyrae variables Name Star name --- HJD Heliocentric Julian day number=1 Heliocentric Julian dates correspond to the start of the V-band exposures. The midpoints of the V, B, and I exposures are, respectively, 2.5, 11.0, and 18.5 min later than this HJD d Vmag V band magnitude mag Bmag B band magnitude mag Imag I band magnitude mag Photometry of the brighter M68 stars Name Star number --- X X coordinate --- Y Y coordinate --- Vmag V magnitude mag B-V B-V color mag V-I V-I color mag Lee Brotzman ADS 10-Oct-199, Patricia Bauer CDS 1995 Feb 16 Walker A.R. awalker@noao.edu Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile AAS CD-ROM series, Volume 3, 1995 J_AJ_108_555.xml Arm structure in normal spiral galaxies. I. Multivariate data for 492 galaxies J/AJ/108/896 J/AJ/108/896 Arm structure in galaxies Arm structure in normal spiral galaxies. I. Multivariate data for 492 galaxies C Magri Astron. J. 108 896 1994 1994AJ....108..896M Infrared sources Photometry Redshifts Spectroscopy Multivariate data have been collected as part of an effort to develop a new classification system for spiral galaxies, one which is not necessarily based on subjective morphological properties. A sample of 492 moderately bright northern Sa and Sc spirals was chosen for future statistical analysis. New observations were made at 20 and 21 cm; the latter data are described in detail here. IRAS fluxes were obtained from archival data. Finally, new estimates of arm pattern randomness and of local environmental harshness were compiled for most sample objects.
KGC basic data UGC Uppsala General Catalogue of Galaxies number --- Name2 Other name --- Sample Code for KGC galaxy subsample number=1 The "sample flag" sample is 'V' for galaxies with m = 13.2 or brighter which are in the Virgo core (within six degrees of M87); it is 'X' for galaxies which are within ten degrees of M87 but which are fainter than m = 13.2; and it is blank otherwise. --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec MajAxis Major diameter arcmin MinAxis Minor diameter arcmin Mag Photographic magnitude, from UGC mag MtypeRSA Morphological type, Revised Shapley-Ames --- MTypeRC2 Morphological type, Second Reference Catalog --- MType Hubble morphological type, UGC --- MType rev Revised Hubble morphological type, UGC --- Raw and corrected diameters and magnitudes UGC UGC number --- MajAxis Major diameter, UGC arcmin MinAxis Minor diameter, UGC arcmin Mag Magnitude, as given in UGC mag D25 Major diameter, 25 blue mag/arcsec2 (25 uB) arcmin n_D25 Note on diameter number=1 The flag for any of the three RC2 photometric parameters is set equal to '*' when that parameter has been directly measured on the RC2 system for a given galaxy. If, instead, the parameter has been estimated based on statistical relationships between UGC and RC2 quantities, then the flag is left blank. --- R25 Axial ratio at 25 uB --- n_R25 Note on ratio number=1 The flag for any of the three RC2 photometric parameters is set equal to '*' when that parameter has been directly measured on the RC2 system for a given galaxy. If, instead, the parameter has been estimated based on statistical relationships between UGC and RC2 quantities, then the flag is left blank. --- BT Total blue magnitude within 25 uB mag n_BT Note on total blue magnitude number=1 The flag for any of the three RC2 photometric parameters is set equal to '*' when that parameter has been directly measured on the RC2 system for a given galaxy. If, instead, the parameter has been estimated based on statistical relationships between UGC and RC2 quantities, then the flag is left blank. --- D0 Corrected blue diameter arcmin BT0 Corrected total blue magnitude mag Raw IRAS data UGC Uppsala General Cat. of Galaxies number --- l_S12 Limit flag on 12um flux density number=1 The flag is set to '<' when S12 represents an upper limit taken from PSC; otherwise it is left blank. (Note that it is left blank for upper limits NOT taken from PSC.) --- S12 Flux density, 12 um Jy e_S12 rms baseline noise, 12 um mJy FWHM12 FWHM angular diameter, 12 um arcmin Code12 Detection code, 12 um number=2 Detection codes are: 0 for nondetections 1 for good detections 2 for marginal detections 3 for improbable detections 4 for PSC/SSSC detections which are probably confused 5 for spirals mapped by Rice et al., 1988, ApJS, 68, 91 6 for unconfused PSC data 7 for unconfused SSSC data 8 for one galaxy (UGC 6962) for which existing IRAS data were not coadded; and -1 for objects not observed by IRAS. See printed article for details. --- S25 Flux density, 25 um Jy e_S25 rms baseline noise, 25 um mJy FWHM25 FWHM angular diameter, 25 um arcmin Code25 Detection code, 25 um number=2 Detection codes are: 0 for nondetections 1 for good detections 2 for marginal detections 3 for improbable detections 4 for PSC/SSSC detections which are probably confused 5 for spirals mapped by Rice et al., 1988, ApJS, 68, 91 6 for unconfused PSC data 7 for unconfused SSSC data 8 for one galaxy (UGC 6962) for which existing IRAS data were not coadded; and -1 for objects not observed by IRAS. See printed article for details. --- S60 Flux density, 60 um Jy e_S60 rms baseline noise, 60 um mJy FWHM60 FWHM angular diameter, 60 um arcmin Code60 Detection code, 60 um number=2 Detection codes are: 0 for nondetections 1 for good detections 2 for marginal detections 3 for improbable detections 4 for PSC/SSSC detections which are probably confused 5 for spirals mapped by Rice et al., 1988, ApJS, 68, 91 6 for unconfused PSC data 7 for unconfused SSSC data 8 for one galaxy (UGC 6962) for which existing IRAS data were not coadded; and -1 for objects not observed by IRAS. See printed article for details. --- S100 Flux density, 100 um Jy e_S100 rms baseline noise, 100 um mJy FWHM100 FWHM angular diameter, 100 um arcmin Code100 Detection code, 100 um number=2 Detection codes are: 0 for nondetections 1 for good detections 2 for marginal detections 3 for improbable detections 4 for PSC/SSSC detections which are probably confused 5 for spirals mapped by Rice et al., 1988, ApJS, 68, 91 6 for unconfused PSC data 7 for unconfused SSSC data 8 for one galaxy (UGC 6962) for which existing IRAS data were not coadded; and -1 for objects not observed by IRAS. See printed article for details. --- New HI parameters for KGC spirals UGC UGC number --- VHel Heliocentric velocity km/s VLG Velocity relative to Local Group barycenter km/s rms rms baseline noise mJy HI HI profile width, 50% mean signal strength km/s VRot Computed rotation velocity km/s SHI Raw HI flux Jy.km/s SHICorr Corrected HI flux Jy.km/s Tel Telescope code number=1 The telescope code (code "C" in the printed article) is 0 for spirals observed with either of the two dual-circular feeds at Arecibo 1 for those observed with the 91 m Green Bank dish 2 for those observed with the Arecibo flat feed. --- Det Detection code number=2 The detection code (code "D" in the printed article) is 0 for nondetections 1 for good detections 2 for marginal detections 3 for confused detections 4 for spirals whose spectra show HI absorption 9 for objects of unknown redshift for which a search in velocity space was unsuccessful. --- Dist Distance Mpc l_log(HIMass) Limit flag on HI mass number=3 The flag is set to '<' when the HI mass which follows is an upper limit, and is left blank otherwise. --- log(HIMass) HI mass solMass l_HIDef Limit flag on HI deficiency number=4 The flag is set to '>' when the HI deficiency which follows it is a lower limit, and is left blank otherwise. --- HIDef HI deficiency --- New HI parameters for non-KGC galaxies UGC UGC number --- Name2 Other name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Sign of declination --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec MajAxis Major diameter, from UGC arcmin MinAxis Minor diameter, from UGC arcmin Mag Magnitude, from UGC mag MType RC2-style morphological type --- VHel Heliocentric velocity km/s VLG Velocity relative to Local Group barycenter km/s rms rms baseline noise mJy HI HI profile width, 50% mean signal strength km/s VRot Computed rotation velocity km/s SHI Raw HI flux Jy.km/s SHICorr Corrected HI flux Jy.km/s Tel Telescope code number=1 The telescope code (code "C" in the printed article) is 0 for spirals observed with either of the two dual-circular feeds at Arecibo 1 for those observed with the 91 m Green Bank dish 2 for those observed with the Arecibo flat feed. --- Det Detection code number=2 The detection code (code "D" in the printed article) is 0 for nondetections 1 for good detections 2 for marginal detections 3 for confused detections 4 for spirals whose spectra show HI absorption o 9 for objects of unknown redshift for which a search in velocity space was unsuccessful. --- Dist Distance Mpc l_log(HIMass) Limit flag on HI mass number=3 The flag is set to '<' when the HI mass which follows is an upper limit, and is left blank otherwise. --- log(HIMass) logarithm of the HI mass solMass l_HIDef Limit flag on HI deficiency number=4 The flag is set to '>' when the HI deficiency which follows it is a lower limit, and is left blank otherwise. --- HIDef HI deficiency --- Compiled data on KGC spirals UGC UGC number --- MType Morphological type (w/bar status) on RC2 system --- LC Luminosity class --- NR Non-randomness (see printed text) --- l_BD Limit flag on BD --- BD Bulge-to-disk diameter ratio --- Dist Distance Mpc log(Diam) logarithm of blue diameter kpc log(LB) logarithm of blue luminosity solLum B-V B-V color mag U-B U-B color mag B-H B-H (near-IR) color mag l_log(HIMass) Limit flag for HI mass number=1 The signs placed before several quantities are '<' for upper limits, '>' for lower limits, ':' for marginal detections, blank otherwise. --- log(HIMass) logarithm of H I mass solMass l_HIDef Limit flag for HIDef number=1 The signs placed before several quantities are '<' for upper limits, '>' for lower limits, ':' for marginal detections, blank otherwise. --- HIDef HI deficiency --- log(VRot) logarithm of rotation velocity km/s l_log(LRad) Limit flag for LRad number=1 The signs placed before several quantities are '<' for upper limits, '>' for lower limits, ':' for marginal detections, blank otherwise. --- log(LRad) logarithm of 20 cm luminosity solLum l_log(LFIR) Limit flag for LFIR number=1 The signs placed before several quantities are '<' for upper limits, '>' for lower limits, ':' for marginal detections, blank otherwise. --- log(LFIR) log of far-IR luminosity solLum l_log(LWarm) Limit flag for LWarm number=1 The signs placed before several quantities are '<' for upper limits, '>' for lower limits, ':' for marginal detections, blank otherwise. --- log(LWarm) log of warm-dust luminosity solLum l_log(DustMass) Limit flag for dust mass number=1 The signs placed before several quantities are '<' for upper limits, '>' for lower limits, ':' for marginal detections, blank otherwise. --- log(DustMass) Logarithm of dust mass solMass l_W-C Limit flag for W-C number=1 The signs placed before several quantities are '<' for upper limits, '>' for lower limits, ':' for marginal detections, blank otherwise. --- W-C Warm/cool dust "color" (see text) --- Env Local environmental harshness (see text) --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 19 Department of Astronomy and National Astronomy and Ionosphere Center, Cornell University, Ithaca, New York 14853 AAS CD-ROM series, Volume 3, 1995 J_AJ_108_896.xml Variable stars in and around the SMC cluster NGC 330 J/AJ/108/932 J/AJ/108/932 Variable stars in the SMC cluster NGC 330 Variable stars in and around the SMC cluster NGC 330 K M Sebo P R Wood Astron. J. 108 932 1994 1994AJ....108..932S Magellanic Clouds Photometry, CCD Stars, variable V and I band CCD images of the SMC cluster NGC 330 have been obtained over an interval of 4 years with the aim of identifying variable stars in and around this rich, young cluster. The search has revealed 22 Cepheid variables, of which 14 are newly discovered. All of these appear to belong to the SMC field population rather than being cluster members. Twenty long-period variables, and nine other variables were identified including two eclipsing variables (one newly discovered), and four close binary stars, two of which show emission lines. The Cepheids indicate that only small to moderate amounts of convective core overshoot (f_ov_<~0.25) occur during the main-sequence phases for stars of mass 2-3M_{sun}_. The Cepheid period-luminosity-color relation obtained from VI photometry, when compared to the theoretical relation of Chiosi, et al. (1993ApJS...86..541C), yields a distance modulus for the short-period Cepheids observed during this study of 18.92 if no overshoot is assumed, or 18.72 if moderate overshoot (f_ov=0.25) is adopted. Only two modes of pulsation are present in this group of Cepheids, most likely they are the fundamental and first overtone.
NGC 330 00 56.2 -72 29
Raw data No Star number --- HJD Heliocentric Julian day for Vmag value d Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag HJD2 Heliocentric Julian day for Imag value d Imag I magnitude mag e_Imag rms uncertainty on I mag mag Lee Brotzman ADS 1994, Patricia Bauer [CDS] 16-Feb-1995 Oct 31 Sebo K.M. <kim@mso.anu.edu.au> Wood P.R. <wood@mso.anu.edu.au> Mount Stromlo and Siding Spring Observatories, Private Bag, Weston Creek PO, A.C.T. 2611 Australia AAS CD-ROM series, Volume 3, 1995 J_AJ_108_932.xml The Globular Cluster System of M81 J/AJ/109/1055 J/AJ/109/1055 Globulars of M81 The Globular Cluster System of M81 J M Perelmuter M Racine Astron. J. 109 1055 1995 1995AJ....109.1055P Clusters, globular Photometry Photometric BVR, morphological, and astrometric information has been obtained on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 <= V <= 21. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8].
Catalogue of objects in the M81 field ID Identification number [PR95] --- RAh Right ascension (2000) h RAm R.A. min RAs R.A. s DE- Declination (always blank) --- DEd Declination (2000) deg DEm Dec. arcmin DEs Dec. arcsec Epoch Mean epoch of observation yr Vmag V magnitude mag B-V B-V color mag V-R V-R color mag N Number of plates object detected upon --- pmGlon Proper motion in galactic longitude mas/yr pmGlat Proper motion in galactic latitude mas/yr pmSig Level of significance of total PM The level of significance of the total proper motion, mu/sig_mu, where mu is the total proper motion = (pmGlon^2 + pmGlat^2)^(1/2) --- CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 03-May-1995 J_AJ_109_1055.xml A Photometric Study of the Globular Cluster M54 and the Sagittarius Dwarf Galaxy: Evidence for Three Distinct Populations J/AJ/109/1086 J/AJ/109/1086 VI Photometry in M54 and Sgr Dwarf Galaxy A Photometric Study of the Globular Cluster M54 and the Sagittarius Dwarf Galaxy: Evidence for Three Distinct Populations A Sarajedini A C Layden Astron. J. 109 1086 1995 1995AJ....109.1086S Clusters, globular Photometry, CCD We present VI CCD color-magnitude diagrams for the globular cluster M54 and the Sagittarius dwarf galaxy. These are used to derive the following quantities: [Fe/H] = -1.79 +/- 0.08 for M54 and [Fe/H] = -0.52 +/- 0.09 for Sagittarius. We find a metallicity dispersion of +/- 0.16 dex in M54, and we infer the possible existence of a [Fe/H] ~ -1.3 component in Sagittarius, which may have a metallicity dispersion as well. The mean reddening in the direction of M54 is E(B-V) = 0.13 +/- 0.02. The distances to M54 and Sagittarius, determined using their horizontal branch magnitudes, are identical to within the uncertainties of existing RR Lyrae luminosity-abundance relations. This, together with positional and radial velocity arguments, suggests that M54 is physically associated with Sagittarius. We note that M54 is substantially brighter than the globular cluster members of the Fornax dwarf spheroidal galaxy, and that the metal abundance of Sagittarius is quite high for its estimated absolute magnitude.
M 54 NGC 6715 C 1851-305 18 55.1 -30 28 ESO 594-4 Sgr Dwarf Galaxy 19 30.0 -17 41
CCD photometry for M54. CCD photometry for Sgr. Star Star number --- Xpos X pixel position pix Ypos Y pixel position pix Vmag V magnitude mag e_Vmag V magnitude error mag V-I V-I color mag e_V-I V-I color error mag Det Number of detections --- CDS 1996 Jan 09 AAS CD-ROM series, Vol. 5, 1995 Lee Brotzman [ADS] 17-Jul-1995 J_AJ_109_1086.xml A determination of the thick disk chemical abundance distribution: implications for galaxy evolution. J/AJ/109/1095 J/AJ/109/1095 Thick Disk Chemical Abundance Distribution A determination of the thick disk chemical abundance distribution: implications for galaxy evolution. G Gilmore R F G Wyse J B Jones Astron. J. 109 1095 1995 1995AJ....109.1095G Effective temperatures Photometry, photographic Stars, distances We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15<=V=<18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or >=12Gyr, and are consistent with a spread to older ages.
Observed and derived data for South Galactic Pole stars Observed and derived data for UK Schmidt Field 117 stars (l, b)=(270, -45) RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Vmag V magnitude mag B-V B-V color index mag V-I V-I color index mag [Fe/H] Metallicity Sun Dist Distance from photometric parallax pc Teff Effective temperature from V-I K Patricia Bauer CDS 1996 Jun 14 Rosie Wyse <wyse@physics.Berkeley.EDU> J_AJ_109_1095.xml CCD Photometry for the Galactic Globular Cluster NGC 6584 J/AJ/109/1112 J/AJ/109/1112 NGC 6584 CCD Photometry for the Galactic Globular Cluster NGC 6584 A Sarajedini W L Forrester Astron. J. 109 1112 1995 1995AJ....109.1112S Clusters, globular Photometry, CCD We present CCD photometry in the B and V passbands for the Galactic globular cluster NGC 6584. The color-magnitude diagram reveals a horizontal branch (HB) populated on both the red and blue sides of the RR Lyrae instability strip. The cluster contains 42 confirmed RR Lyrae variables, and we find an additional 56 stars which are possible RR Lyraes. The mean magnitude of the RR Lyraes on our CCD frames is combined with that of the nonvariable stars to yield <V(HB)> = 16.53 +/- 0.03. Using a polynomial fit to the cluster giant stars, we derive the color of the giant branch at the level of the HB to be (B-V)g = 0.89 +/- 0.02. Our photometry has also been used to isolate the red giant branch "clump," which forms when stars pause and sometimes reverse their course as they evolve up the giant branch. Its luminosity is primarily dependent upon the cluster metallicity, and we have used this fact to derive a metallicity of [Fe/H] = -1.44 +/- 0.16 for NGC 6584. Coupled with the color of the giant branch given above, this yields a cluster reddening of E(B-V) = 0.07 +/- 0.04. To the extent that our photometry can be used to study the age of NGC 6584, we find it to be comparable to M3, which is not surprising given their similar HB morphologies. The color-magnitude diagram also exhibits a significant population of blue straggler stars. From a comparison of the blue straggler radial distribution to that of the subgiant stars with similar V magnitudes, we find that the blue stragglers are more centrally concentrated than the subgiants, indicative of a higher mass for the blue stragglers.
NGC 6584 18 18.6 -52 13
CCD photometry for NGC 6584 Star Star number --- Xpos X pixel position pix Ypos Y pixel position pix Vmag V magnitude mag e_Vmag V magnitude error mag B-V B-V color mag e_B-V B-V color error mag Det Number of detections --- CDS 1996 Jan 09 AAS CD-ROM series, Vol. 5, 1995 Lee Brotzman [ADS] 17-Jul-1995 J_AJ_109_1112.xml Infrared Array Photometry of Metal Rich Globular Clusters. II. Liller 1 -- The Most Metal Rich Cluster? J/AJ/109/1154 J/AJ/109/1154 JHK Photometry of Liller 1 Infrared Array Photometry of Metal Rich Globular Clusters. II. Liller 1 -- The Most Metal Rich Cluster? J A Frogel L E Kuchinski G P Tiede Astron. J. 109 1154 1995 1995AJ....109.1154F J/AJ/109/1131 : Paper I: clusters NGC 5927, Terzan 2, NGC 6712, NGC 6838 J/AJ/110/2844 : Paper III: clusters M 71, NGC 5927, NGC 6624, NGC 6440, NGC 6712 Clusters, globular Photometry, infrared We present the first color-magnitude diagram of Liller 1, a globular cluster with an angular separation of only 5 deg from the galactic center and a latitude of 0.2 deg. We estimate a metallicity for this cluster of [Fe/H] = +0.25 +/- 0.3 based on the slope of Liller 1's giant branch in the near-infrared. This implies that Liller 1 is the most metal rich galactic globular cluster known. Any reasonable uncertainty in the age of the cluster will not affect our method for deriving the metallicity. We also conclude that for Liller 1 E(J-K) = 1.70 +/- 0.06 (or A_V ~ 9.5) and (m-M)0 = 14.68 +/- 0.23. The atypical JHK colors of the Liller 1 stars, the extreme slope of its giant branch, and its physical closeness to the galactic center raise the question of whether it is a normal globular cluster or if its formation and evolution have been strongly influenced by its proximity to the galactic center.
C 1730-333 Liller 1 17 33 24.0 -33 23 16
Liller 1 data ID ID number --- Xpos X coordinate on frame pix Ypos Y coordinate on frame pix Kmag Observed K magnitude mag J-K Observed J-K color mag H-K Observed H-K color mag Ring Ring designation Cluster Center at x=80, y=5 (pixels), scale = 0.52 arcsec/pixel I = R < 40 pixels (21 arcsec) from cluster center II = 40 pixels (21 arcsec) < R < 60 pixels (31 arcsec) III = 60 pixels (31 arcsec) < R < 110 pixels (57 arcsec) IV = R > 110 pixels (57 arcsec) --- Code Code for data set 3 = 3sec exposure, 10 = 10sec exposure A3 = 3sec good seeing exposure, AL = good seeing, long exposure --- Note Notes, NO = DoPHOT error > 0.06 mag --- CDS 1995 Jul 11 AAS CD-ROM series, Vol. 4, 1995 Lee Brotzman [ADS] 03-May-1995 J_AJ_109_1154.xml O I Lambda 7774 Absorption as a Tracer of Streams and Disks in Nondegenerate Binary Stars J/AJ/109/1269 J/AJ/109/1269 Streams and Disks in Binary Stars O I Lambda 7774 Absorption as a Tracer of Streams and Disks in Nondegenerate Binary Stars P B Etzel E C Olson M C Senay Astron. J. 109 1269 1995 1995AJ....109.1269E Binaries, eclipsing Equivalent widths Radial velocities We propose a new spectroscopic approach for observing circumstellar matter in binary stars, based on the neutral oxygen lambda 7774 absorption lines. We present oxygen equivalent widths and radial velocities in 20 nondegenerate eclipsing binaries. We note limitations and advantages of using this line to trace circumstellar matter in binary systems, and confirm the presence of streams and rotating accretion disks in a number of short- and long-period Algol systems. We discuss evidence for geometrically thick disks, and describe a small radial infall superimposed on disk rotation in most long-period systems. We speculate that infall may be related to viscous dissipation in disks. We emphasise the great sensitivity of lambda 7774 in studying the kinematics of circumstellar matter in many nondegenerate binary stars.
Equivalent widths and radial velocities Name Variable star name --- UT UT date and time of observation --- HJD Heliocentric Julian Date of observation d Phase Phase --- EW Absorption equivalent width 0.1nm RV Radial velocity km/s CDS 1995 Jul 11 AAS CD-ROM series, Vol. 4, 1995 Lee Brotzman [ADS] 03-May-1995 J_AJ_109_1269.xml Triton stellar occultation candidates: 1995-1999 J/AJ/109/1352 J/AJ/109/1352 Stellar occultation candidates Triton stellar occultation candidates: 1995-1999 S W McDonald J L Elliot Astron. J. 109 1352 1995 1995AJ....109.1352M J/AJ/104/862 : Stellar occultation candidates (McDonald+ 1992) Occultations Positional data We have completed a search for candidates for stellar occultations by Triton over the years 1995-1999 CCD strip scan images provided star positions in the relevant sky area to a depth of about 17.5Rmag. Over this time period, we find that Triton passes within 1.0arcsec of 75 stars. Appulses with geocentric minimum separations of less than 0.35arcsec will result in stellar occultations, but further astrometry and photometry is necessary to refine individual predictions for identification of actual occultations. Finder charts are included to aid in further studies and prediction refinement. The two most promising potential occultations, Tr176 and Tr180, occur in 1997.
Possible occultations by Triton ID Star name --- AppDate Date of the closest approach "DD/MM/YY" Apph UT time of the closest approach h Appm UT time of the closest approach min SepMin Minimum separation of the closest approach arcsec PA Position angle of Triton relative to the star at the time of the closest approach (North to East) deg Rmag CCD magnitude mag Vel Velocity of the occultation shadow km/s l_S/N Limit flag on S/N --- S/N Signal to noise ratio number=1 The S/N for the light curve has been calculated for an averaging interval of 20km (the approximate scale height of Triton's atmosphere), based on the S/N of 30.3 achieved for Tr60 by Elliot et al. (1993BAAS...25.1106E) with the 0.9m KAO telescope with a CCD photometer (no filter). Background limited performance has been assumed, which may lead to an overestimate of S/N for the brightest sources. Potential observers should evaluate the S/N for their own photometric equipment. --- Dist Angular distance between Triton and the Sun deg RAh Right ascension (J2000) of the star h RAm Right ascension (J2000) of the star min RAs Right ascension (J2000) of the star s DE- Declination sign --- DEd Declination (J2000) of the star deg DEm Declination (J2000) of the star arcmin DEs Declination (J2000) of the star arcsec Elon Sub_Earth longitude of the star at the mid-time of the event deg Strip Strip numbers on which an image of the candidate star was measured --- James Marcout, Patricia Bauer CDS 1997 Apr 01 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_109_1352.xml Moderate-resolution spectral standards from 560 to 900 nm J/AJ/109/1379 J/AJ/109/1379 Praesepe & M 67 spectral standards Moderate-resolution spectral standards from 560 to 900 nm L E Allen K M Strom Astron. J. 109 1379 1995 1995AJ....109.1379A Clusters, open MK spectral classification Photometry We present a grid of stellar classification spectra of moderate resolution (R~1500) in the range lambda lambda 5600-9000A, compiled from high signal-to-noise spectra of 275 stars, most in the open clusters Praesepe and M 67. The grid covers dwarfs from types B8 through M5, giants from G8 through M7, and subgiants from F5 through K0. We catalog atomic and molecular absorption features useful for stellar classification, and demonstrate the use of luminosity-sensitive features to distinguish between late-type dwarf and giant stars.
M 67 NGC 2682 08 50.4 +11 49 M 44 Praesepe NGC 2632 08 40.4 +19 40
Spectral standards in Praesepe Spectral standards in M 67 ID Identification number number=1 In table1, ID from Jones and Stauffer (1991AJ....102.1080J) In table2, ID from Sanders (1977A&AS...27...89S) --- n_ID * when spectrum plotted number=2 *: spectrum plotted in Figure 3 for table1, in Figure 5 for table2. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Sp Adopted spectral type --- Vmag V magnitude mag B-V B-V color index mag V-I V-I color index mag Prob Probability of membership number=3 In table1, Prob from Jones and Stauffer (1991AJ....102.1080J) In table2, Prob from Girard et al. (1989AJ.....98..227G) % r_Vmag BVI photometry reference number=4 0: BVI photometry from Jones and Stauffer (1991AJ....102.1080J) 1: BV photometry from Girard et al. (1989AJ.....98..227G) 2: BVI photometry from Montgomery et al. (1993) <J/AJ/106/181> --- Notes Notes number=5 In table1: Ab = Abt (1986PASP...98..307A) Ba = Barbier (1963POHP....6...36B) BB = Boesgaard and Budge (1988ApJ...332..410B) Bi = Bidelman (1956PASP...68..318B) Bo = Bolte (1991ApJ...376..514B) CB = Crawford and Barnes (1969AJ.....74..818C) CGal = Corbally and Garrison (1986AJ.....92...90C) CGb = Corbally and Garrison (1983JRASC..77...28C) Jo = Johnson (1952ApJ...116..640J) Po = Popper (1948ApJ...108..490P) Re = Rebeirot (1966POHP....8...24R) RS = Randich and Schmitt (1994) Cat. <J/A+A/298/115> SS = Soderblom and Stauffer (1984AJ.....89.1543S) St = Stauffer (1982PASP...94..678S) Up = Upgren et al. (1979AJ.....84.1586U) Wi = Wilson (1963ApJ...138..832W) In table2: Identification cross references: F: Fagerholm ID (1906ArMAF...2s...1F) RGO: Royal Greenwich Observatory ID S: Sandage ID Previously published spectral types from: BB: Burbidge and Burbidge (1959ApJ...129..513B) Pe: Pesch (1967ApJ...148..781P) Po: Popper (1954AJ.....59..445P) --- Additional giants Name Star name --- n_Name * when spectrum plotted in Figure 3 --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Sp Spectral type --- Spectral features Lambda Wavelength 0.1nm n_Lambda Separator, '-' for interval --- Lambda2 Second wavelength 0.1nm n_Lambda2 Separator --- Lambda3 Third wavelength 0.1nm Ident Identification --- Notes Notes --- Ref References number=1 1: Torre-Dodgen & Weaver (1993) <III/181> 2: Kirkpatrick et al. (1991ApJS...77..417K) --- James Marcout, Patricia Bauer CDS 1996 Oct 01 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_109_1379.xml The redshift-space neighbourhoods of 36 loose groups of galaxies. I. The data. J/AJ/109/1458 J/AJ/109/1458 Neighborhoods of 36 loose groups of galaxies The redshift-space neighbourhoods of 36 loose groups of galaxies. I. The data. M Ramella M J Geller J P Huchra J R Thorstensen Astron. J. 109 1458 1995 1995AJ....109.1458R galaxies: groups We have selected 36 loose groups of galaxies from Ramella et al. 1989, with at least five members, and with mean redshift cz>3200km/s. These groups all lie within the first two "slices" of the CfA redshift survey <VII/164> (RA between 8h and 17h, DE between 2655.5 and 38.5 degrees). For each of these groups, we define the "redshift-space neighbourhood" as a region centered on the group coordinates and delimited by a circle of projected radius 1.5xh^-1^ Mpc on the sky, and by a velocity interval of 3000km/s. Table 2 lists the positions, magnitudes, radial velocities (cz) and their errors, for the members of the groups published in RGH89. Coordinates and magnitudes are from Zwicky's CGCG <VII/4>. Unpublished redshifts are marked with an asterisk in the last column. Table 3 lists galaxies within 1.5Mpc (assuming H0=100) and +/-1500 km/s from the centers of the groups in redshift space. Magnitudes and positions are from the Zwicky-Nielsen merged catalog. Some coordinates are better coordinates than Zwicky's, some come from compilations of redshift data that we have used to complement our measurements. Unpublished redshifts are marked with an asterisk in the last column. In this table some galaxies appear twice because a few groups do overlap. We listed the galaxies in common under the labels of both groups.
The original group members in RGH89 Additional galaxies RGH89 Group number (Table 5 from Ramella et al, 1989) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec B(0) Magnitude in the Zwicky system mag cz Heliocentric velocity km/s e_cz Mean error on cz km/s n_cz The asterisk indicates a new measurement (unpublished redshift) --- table2.tex plain TeX version of table2 table3.tex plain TeX version of table3 Francois Ochsenbein CDS 1995 Jul 21 Massimo Ramella <ramella@oat.ts.astro.it> J_AJ_109_1458.xml Optical spectroscopy of radio galaxies in Abell clusters. I. Redshifts and emission-line properties. J/AJ/109/14 J/AJ/109/14 Optical spectroscopy of Abell clusters. I. Optical spectroscopy of radio galaxies in Abell clusters. I. Redshifts and emission-line properties. F N Owen M J Ledlow W C Keel Astron. J. 109 14 1995 1995AJ....109...14O VIII/29 : 1400-MHz Survey of 1478 Abell Galaxy Clusters (Owen+ 1982) J/AJ/109/853 : VLA survey of Abell clusters. IV. (Ledlow+ 1995) J/AJ/110/1959 : VLA survey of Abell clusters. V. (Ledlow+ 1995) Owen et al., Paper II. 1996AJ....111...53O Clusters, galaxy Galaxies, radio Redshifts Spectroscopy We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.
Spectral parameters for radio galaxies in Abell clusters Spectral parameters for foreground and background radio identifications ACO Abell number --- IAU IAU name --- m_IAU Multiplicity index on IAU --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec z Redshift --- e_z rms uncertainty on z --- Run Run numbers number=1 Summary of observing runs ---------------------------------------------------------------------- No Date CCD Grating Lines/mm {AA}/pix Wavelength range ---------------------------------------------------------------------- 1 28/01-31/01/92 Ti 800x800 09 300 2.47 3560-5525 2 26/05-29/05/92 Ford 3x1 K 240 500 1.49 3476-7725 3 25/09-28/09/92 Ford 3x1 K 240 500 1.49 3160-7725 4 17/11-20/11/92 Ford 3x1 K 09 300 2.44 3425-7730 5 24/04- 2/05/93 Ford 3x1 K 09 300 2.44 3430-7695 --- l_EW1 Limit flag on EW1 --- EW1 H{alpha}+[NII] equivalent width 0.1pm e_EW1 rms uncertainty on EW1 0.1pm l_EW2 Limit flag on EW2 --- EW2 O[II]3727{AA} equivalent width 0.1pm e_EW2 rms uncertainty on EW2 0.1pm Note Notes number=2 1 : Combined emission and absorption line redshift. 2 : Emission line redshift. 3 : Absorption line redshift measured manually. 4 : Star. 5 : Uncertain but not galaxy at cluster redshift. 6 : Spiral 7 : Seyfert-like spectrum --- James Marcout, Patricia Bauer CDS 1997 Jul 29 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_109_14.xml Near-Infrared Surface Photometry and Morphology in Virgo Cluster Spiral Galaxy Nuclear Regions J/AJ/109/1608 J/AJ/109/1608 Near-IR Surface Photometry in Virgo Spirals Near-Infrared Surface Photometry and Morphology in Virgo Cluster Spiral Galaxy Nuclear Regions B J Rauscher Astron. J. 109 1608 1995 1995AJ....109.1608R Photometry, infrared Photometry, surface The tables contain elliptical isophotes interactively fit to the K images using the Space Telescope Science Data Analysis Software (STSDAS) task ELLIPSE. This paper presents very high spatial resolution (seeing 0.75 arcsec FWHM) K band surface photometry of 15 Virgo cluster spiral galaxy nuclear regions (radii <1 kpc). It presents B and I band CCD images of 13 of these galaxies. The goals of the study were: (1) to begin to establish a K band baseline of normal spiral galaxy nuclear regions against which peculiar galaxies may be compared, (2) to provide better constraints on N-body models, and (3) to complement near-infrared studies of large scale structure in spiral galaxies with very high resolution imaging of the important nuclear regions. The principal findings are: (1) between 1/4 and 1/3 of these nuclear regions show K band evidence of triaxiality, (2) approximately 1/2 of these galaxies have axisymmetric nuclear regions, and (3) NGC 4321 has a bar that is not detectable in the optical images.
NGC 4192 M 98 12 13.7 +14 53 NGC 4216 12 15.9 +13 09 NGC 4254 M 99 12 18.8 +14 25 NGC 4303 M 61 12 21.9 +04 28 NGC 4321 M 100 12 22.9 +15 49 NGC 4394 12 25.9 +18 13 NGC 4438 12 27.7 +13 00 NGC 4457 12 29.0 +03 34 NGC 4501 M 88 12 31.9 +14 25 NGC 4535 12 34.3 +08 11 NGC 4548 M 91 12 35.4 +14 29 NGC 4567 12 36.5 +11 15 NGC 4568 12 36.5 +11 14 NGC 4639 12 42.9 +13 16 NGC 4651 12 43.8 +16 24
NGC 4192 K band surface photometry NGC 4216 K band surface photometry NGC 4254 K band surface photometry NGC 4303 K band surface photometry NGC 4321 K band surface photometry NGC 4394 K band surface photometry NGC 4438 K band surface photometry NGC 4457 K band surface photometry NGC 4501 K band surface photometry NGC 4535 K band surface photometry NGC 4548 K band surface photometry NGC 4567 K band surface photometry NGC 4568 K band surface photometry NGC 4639 K band surface photometry NGC 4651 K band surface photometry MajAxis Semi-major axis arcsec SurfBr Surface brightness mag/arcsec2 e_SurfBr Surface brightness relative error mag/arcsec2 Ellip Ellipticity --- e_Ellip Ellipticity probable error --- PA Position angle, north through east deg e_PA Position angle probable error deg CDS 1995 Jul 11 AAS CD-ROM series, Vol. 4, 1995 Lee Brotzman [ADS] 04-May-1995 J_AJ_109_1608.xml Star formation in dwarf irregular galaxies: NGC 6822. J/AJ/109/173 J/AJ/109/173 BVR photometry of NGC 6822 Star formation in dwarf irregular galaxies: NGC 6822. G Marconi M Tosi L Greggio P Focardi Astron. J. 109 173 1995 1995AJ....109..173M J/AJ/105/894 : Star formation in DDO 210 and NGC 3109 (Greggio+ 1993) Galaxies, photometry Photometry, CCD Our proposed method to study the star-formation histories in nearby irregulars is here applied to NGC 6822. To this purpose we have obtained accurate CCD photometry of three regions in the galaxy, reaching V=23.5 with the required accuracy of {sigma}_BVR_<=0.1mag. Major information on the stellar populations, star-formation rates, and initial mass functions of these regions in the last 1Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. We find that in the last 1Gyr the star-formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods, and that the initial mass function exponent a is in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 6822 appear to contain different stellar populations. The preferred star formation regime for region A is a continuous activity coupled with a moderately flat {alpha}. For region C, instead, our best models suggest a discontinuous star formation and a moderately steep {alpha}. NGC 6822 is the last object of our original sample of five nearby irregulars. We can then draw the scenario resulting from this sample: most of the observed fields appear to have experienced a gasping regime of star formation, with average exponent {alpha}=2.35 for the initial mass function. Despite their small sizes, the majority of the sample galaxies contain different stellar populations in different regions.
NGC 6822 19 44 56.0 -14 48 06
Principal parameters of the selected stars of NGC 6822 Region NGC 6822 region --- Star Star number in the region --- Xpos X position number=1 The field are centered at: RA(1950)=19h42m07s, DE(1950)=-14{deg}58'24" for field A RA(1950)=19h42m15s, DE(1950)=-14{deg}55'54" for field B RA(1950)=19h42m07s, DE(1950)=-14{deg}53'23" for field C North is down, East is right, 1 pix = 0.17" pix Ypos Y position number=1 The field are centered at: RA(1950)=19h42m07s, DE(1950)=-14{deg}58'24" for field A RA(1950)=19h42m15s, DE(1950)=-14{deg}55'54" for field B RA(1950)=19h42m07s, DE(1950)=-14{deg}53'23" for field C North is down, East is right, 1 pix = 0.17" pix Vmag V magnitude mag B-V B-V colour index mag V-R V-R colour index mag James Marcout, Patricia Bauer CDS 1997 Sep 16 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_109_173.xml H-Alpha Measurements for Cool Giants J/AJ/109/1797 J/AJ/109/1797 H-Alpha Measurements for Cool Giants H-Alpha Measurements for Cool Giants J A Eaton Astron. J. 109 1797 1995 1995AJ....109.1797E Equivalent widths Stars, giant The H-alpha line in a cool star is usually an indication of the conditions in its chromosphere. I have collected H-alpha spectra of many northern G-M stars, which show how the strength and shape of the H-alpha line change with spectral type. These observations detect surprisingly little variation in absorption-line depth (Rc ~ 0.23 +/- 0.08), linewidth (FWHD ~ 1.44 +/- 0.22 A), or equivalent width (EW ~ 1.12 +/- 0.17 A) among G5-M5 III giants. Lines in the more luminous stars tend to be broader and stronger by 30%-40% than in the Class III giants, while the H-alpha absorption tends to weaken among the cooler M giants. Velocities of H-alpha and nearby photospheric lines are the same to within 1.4 +/- 4.4 km/s for the whole group. To interpret these observations, I have calculated H-alpha profiles, Ly-alpha strengths and [C II] strengths for a series of model chromospheres representing a cool giant star like Alpha Tau. Results are sensitive to the mass of the chromosphere, to chromospheric temperature, to clumping of the gas, and to the assumed physics of line formation. The ubiquitous nature of H-alpha in cool giants and the great depth of observed lines argue that chromospheres of giants cover their stellar disks uniformly and are homogeneous on a large scale. This is quite different from conditions on a small scale: To obtain a high enough electron density with the theoretical models, both to explain the excitation of hydrogen and possibly also to give the observed [C II] multiplet ratios, the gas is probably clumped. The 6540-6580 A spectra of 240 stars are plotted in an Appendix, which identifies the date of observation and marks positions of strong telluric lines on each spectrum. Section 2 assesses the effects of telluric lines and estimates that the strength of scattered light is ~5% of the continuum in these spectra. Table 1 gives the measurements of H-alpha as well as equivalent widths of two prominent photospheric lines, Fe I lambda 6546 and Ca I lambda 6572, which strengthen with advancing spectral type.
Measurements of H-alpha in Red Giants Star Bright Star <V/50> (HR) star number --- Name Other name --- Note Table note letter a. Observed with Kitt Peak coude feed telescope only b. from Kurucz et al. 1984, Solar Flux Atlas from 296 to 1300 nm --- Sp Spectral type --- Vmag V magnitude mag B-V B-V magnitude mag Rc Residual intensity of H-alpha line --- l_FWHD FWHD limiting character --- FWHD Full-width of H-alpha at half-depth 0.1nm l_EW EW limiting character --- EW Equivalent width of H-alpha 0.1nm dRV Diff. in radial velocity between H-alpha and strong metallic lines km/s EW_FeI Equivalent width of Fe I lambda 6546 0.1nm n_EW_FeI Possible telluric line contamination A "T" indicates that the equivalent widths possibly are contaminated by telluric absorption lines. See the printed paper, section 2 for a discussion of the analysis for marking the equivalent widths as possibly contaminated. --- EW_CaI Equivalent width of Ca I lambda 6572 0.1nm n_EW_CaI Possible telluric line contamination --- table1.tex TeX version of table1.tex CDS 1995 Jul 11 AAS CD-ROM series, Vol. 4, 1995 Lee Brotzman [ADS] 04-May-1995 J_AJ_109_1797.xml Amendment of our method for deriving stellar membership of an open cluster J/AJ/109/1903 J/AJ/109/1903 Membership to cluster IC 4756 Amendment of our method for deriving stellar membership of an open cluster M Missana N Missana Astron. J. 109 1903 1995 1995AJ....109.1903M Clusters, open Our method for determining statistically the members of an open cluster by means of the proper motions (Missana et al., (1990AJ....100.1850M) is amended and its validity is verified by applying it to the cluster IC 4756 with the data given by Herzog et al. (1975A&AS...19..211H), adding nothing to their results. In the computation of the dispersion ellipses of the samples and of the {chi}^2^ for deriving the significance levels, the weights of the proper motions have been taken into account. The results obtained by the criterion of the {chi}^2^ and those obtained by Herzog et al. by the criterion of the maximum likelihood of Sanders (1971A&A....14..226S) are concordant.
IC 4756 C 1836+054 18 39.0 +05 28
Membership probabilities to IC 4756 Star Number of the star in Herzog et al. (1975A&AS...19..211H) --- Mi Membership probability P(C\A). number=1 Probable member if P(C/A)>=0.5. See Missana et al., 1990AJ....100.1850M, for more details. --- n_Mi * and & indicate that the star belongs to the set of 174 and 109 cluster members respectively. --- HS Membership probability according to Herzog et al. ((1975A&AS...19..211H) --- MF Cluster member (M) or field star (F) as per phot. estimates by Herzog et al. --- B B: Blue straggler. --- James Marcout, Patricia Bauer CDS 1997 Apr 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_109_1903.xml Catalogue of Galactic globular-cluster surface-brightness profiles J/AJ/109/218 J/AJ/109/218 Catalogue of globular cluster profiles Catalogue of Galactic globular-cluster surface-brightness profiles S C Trager I R King S Djorgovski Astron. J. 109 218 1995 1995AJ....109..218T II/117 : Catalog of UBVRI Photometry of Globular Clusters (Peterson 1986) VII/151 : Structure Parameters of Galactic Globular Clusters (Webbink 1985) Clusters, globular Photometry, surface The data for individual objects are in tables file. The header information, which provides the Chebyshev and power-of-x coefficients, for each cluster are in tables.hdr file We present a catalogue of surface-brightness profiles (SBPs) of 125 Galactic globular clusters, the largest such collection ever gathered. The SBPs are constructed from generally inhomogeneous data, but are based heavily on the Berkeley Globular Cluster Survey of Djorgovski & King. All but four of the SBPs have photometric zero points. We derive central surface brightnesses, King-model concentrations, core radii, half-light, and other fraction-of-light radii where data permit, and we briefly discuss their use.
Data points for SBPs Name Cluster name --- logRad Log of radius of surface brightness meas. arcsec muV Meas. surface brightness at r, in V mags. mag/arcsec2 muVf Fitted surface brightness at r, from Chebyshev fit mag/arcsec2 Resid Residual of Chebyshev fit at r, muV-muVf mag/arcsec2 Weight Weight of data point in Chebyshev fit --- DataSet Data set name The CCD data follow a naming convention: "C" stands for data taken at CTIO; e.g. "CRB1" stands for the first "B" image from the CTIO 1.5m reflector with the RCA chip. "L" stands for the Lick 1 m Nickel reflector: these datasets are labeled as, e.g. "LTR-B", the second frame from the Lick Nickel reflector, taken with the T1 chip through the Spinrad "R" filter. See Sec. 2.1 of printed paper for details of chips and filters. "DJB2" stands for the second "B" image taken by Djorgovski. For Terzan 5, "I" refers to an I-band image from CTIO kindly provided by Dr. T. Armandroff. "UPGA.4" means the first ("A") ultraviolet ("U") plate used for photographic photometry ("PG") of the cluster in question. "SCAN" data are scanning photoelectric photometry. "ANN" data are centered-aperture photoelectric photometry. Photographic star counts are referenced by plate number; see caption to Figure 2 in printed paper for references. --- CDS 1995 Jul 10 AAS CD-ROM series, Vol. 4, 1995 Lee Brotzman [ADS] 26-Apr-1995 J_AJ_109_218.xml Radio identifications of extragalactic IRAS sources J/AJ/109/2318 J/AJ/109/2318 Extragalactic IRAS sources Radio identifications of extragalactic IRAS sources J J Condon E Anderson J J Broderick Astron. J. 109 2318 1995 1995AJ....109.2318C II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989) VIII/14 : 87GB Catalog of radio sources (Gregory et al., 1991) Infrared sources Radio sources Extragalactic sources detected at lambda=60um were selected from the IRAS Faint Source Catalog, Version 2 <II/156> by the criterion S(60um)>=S(12um). They were identified by position coincidence with radio sources stronger than 25mJy at 4.85GHz in the 6.0sr declination band 0deg<Dec.<+75deg (excluding the 0.05sr region 12h40m<R.A.<14h40m, 0deg<Dec.<+5deg) and with radio sources stronger than 80mJy in the 3.4sr area 0h<R.A.<20h, -40deg<Dec.<0deg (plus the region 12h40m<R.A.<14h40m, 0deg<Dec.<+5deg). Fields containing new candidate identifications were mapped by the VLA at 4.86GHz with about 15" FWHM resolution. Difficult cases were confirmed or rejected with the aid of accurate (sigma~1") radio and optical positions. The final sample of 354 identifications in Omega=9.4sr is reliable and large enough to contain statistically useful numbers of radio-loud FIR galaxies and quasars. The logarithmic FIR/radio flux ratio parameter q can be used to distinguish radio sources powered by "starbursts" from those powered by "monsters." Starbursts and normal spiral galaxies in a lambda=60um flux-limited sample have a narrow (sigma_q=0.14+/-0.01) q distribution with mean <q>=2.74+/-0.01, and none have "warm" FIR spectra [alpha(25um, 60um)<1.5]. The absence of radio-quiet (but not completely silent) blazars indicates that nearly all blazars become optically thin at frequencies nu<~100GHz. Nonthermal sources with steep FIR/optical spectra and dust-embedded sources visible only at FIR and radio wavelengths must be very rare.
Infrared and radio data IRAS IRAS FSC2 name FHHMM.M+DDMM --- RAh IRAS FSC2 B1950 right ascension h RAm IRAS FSC2 B1950 right ascension min RAs IRAS FSC2 B1950 right ascension s DE- IRAS FSC2 B1950 Declination sign --- DEd IRAS FSC2 B1950 Declination deg DEm IRAS FSC2 B1950 Declination arcmin DEs IRAS FSC2 B1950 Declination arcsec l_S12 S12 upper limit symbol --- S12 IRAS 12 um flux density number=1 Flux densities at 12, 25, 60, and 100um from (in descending order of preference) the IRAS Catalog of Large Optical Galaxies (Rice et al. <VII/109>) the revised IRAS Bright Galaxy Sample (Soifer et al. 1989AJ.....98..766S) the IRAS Small Scale Structures Catalog (Helou & Walker <VII/73>) and the FSC2 itself (Moshir et al. <II/156>) Jy l_S25 S25 upper limit symbol --- S25 IRAS 25 um flux density number=1 Flux densities at 12, 25, 60, and 100um from (in descending order of preference) the IRAS Catalog of Large Optical Galaxies (Rice et al. <VII/109>) the revised IRAS Bright Galaxy Sample (Soifer et al. 1989AJ.....98..766S) the IRAS Small Scale Structures Catalog (Helou & Walker <VII/73>) and the FSC2 itself (Moshir et al. <II/156>) Jy l_S60 S60 upper limit symbol --- S60 IRAS 60 um flux density number=1 Flux densities at 12, 25, 60, and 100um from (in descending order of preference) the IRAS Catalog of Large Optical Galaxies (Rice et al. <VII/109>) the revised IRAS Bright Galaxy Sample (Soifer et al. 1989AJ.....98..766S) the IRAS Small Scale Structures Catalog (Helou & Walker <VII/73>) and the FSC2 itself (Moshir et al. <II/156>) Jy l_S100 S100 upper limit symbol --- S100 IRAS 100 um flux density number=1 Flux densities at 12, 25, 60, and 100um from (in descending order of preference) the IRAS Catalog of Large Optical Galaxies (Rice et al. <VII/109>) the revised IRAS Bright Galaxy Sample (Soifer et al. 1989AJ.....98..766S) the IRAS Small Scale Structures Catalog (Helou & Walker <VII/73>) and the FSC2 itself (Moshir et al. <II/156>) Jy RAh2 Radio B1950 right ascension h RAm2 Radio B1950 right ascension min RAs2 Radio B1950 right ascension s DE-2 Radio B1950 Declination sign --- DEd2 Radio B1950 Declination deg DEm2 Radio B1950 Declination arcmin DEs2 Radio B1950 Declination arcsec S4.85GHz 4.85 GHz flux density number=2 4.85GHz flux density from the 87GB source catalog (Gregory & Condon 1991 <VIII/14>) or measured from the 87GB or 90GB sky maps, and corrected for strong confusing sources visible in the 4.86GHz VLA maps. mJy Optical data and derived quantities IRAS IRAS FSC2 name FHHMM.M+DDMM --- Name Common name --- RAh Optical B1950 right ascension h RAm Optical B1950 right ascension min RAs Optical B1950 right ascension s DE- Optical B1950 Declination sign --- DEd Optical B1950 Declination deg DEm Optical B1950 Declination arcmin DEs Optical B1950 Declination arcsec Type Identification morphology from the UGC --- mp Apparent photographic magnitude mag Dist Distance for H_0=50km/s/Mpc number=1 Distance from the Revised Shapley-Ames Catalog (Sandage & Tammann 1981 <VII/51>) or the Hubble distance based on H_0=50km/s/Mpc, q0=1/2. Mpc l_q Upper limit symbol for q --- q Log FIR/radio flux-ratio parameter, 4.85 GHz --- alp Radio spectral index between 1.4 and 5GHz --- l_alp_IR Lower limit symbol for alp_IR --- alp_IR FIR spectral index between 25-60 um --- ES Energy source, S = stars, M = monster --- CDS 1996 Oct 23 AAS CD-ROM series, Vol. 5, 1995 Lee Brotzman [ADS] 17-Jul-1995 J_AJ_109_2318.xml Imaging and spectroscopic observations of the Case Survey blue/emission-line galaxies. J/AJ/109/2376 J/AJ/109/2376 Case blue/emission-line galaxies Imaging and spectroscopic observations of the Case Survey blue/emission-line galaxies. J J Salzer J W Moody J L Rosenberg S A Gregory M V Newberry Astron. J. 109 2376 1995 1995AJ....109.2376S Galaxies, photometry Photometry, CCD Radial velocities We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.
The Case galaxies-sample properties. CG Case Survey number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec l_Vmag Limit flag on Vmag --- Vmag Apparent magnitude estimate mag SpCode Spectral code number=1 The first code is an estimate of the color of the continuum. When the code is absent, there is a blank in column 28 mb: moderate blue b: (blue), means that the UV continuum is enhanced y: (yellow), means that the spectrum looks like a more typical F- or G-type galaxy The second and first parameters are the strength of the [OII] and [OIII] lines, respectively. If the [OII] line is not present, there is a blank after the continuum color: vs: very strong s: strong m: medium strength w: weak A ? after the value means that the detection was questionable --- Bmag B magnitude mag n_Bmag Note on Bmag number=2 #: Denotes apparent magnitudes obtained under slightly non-photometric conditions. --- r_Bmag Reference for B magnitude number=3 1: MDM CCD photometry 2: CPO CCD photometry 3: CGCG magnitudes modified as specified by Kron & Shane (1976Ap&SS..39..401K) 4: Case survey list magnitudes modified using the mean offset between Bmag and mvis (Bmag=mvis+0.25) --- DiamA Angular diameter arcsec RV Radial velocity corrected to the velocity centroid of the local group km/s BMAG Absolute B magnitude mag DiamL Linear diameter kpc Names Other names number=4 U = UGC (Nilson 1973, Cat. <VII/26>) N = NGC (See Cat. <VII/1>) I = IC (Dreyer 1888, 1895, 1908, Cat. <VII/118>) Mk = Markarian (1981, Cat. <VII/172>) Wa = Wasilewski (1983ApJ...272...68W) Haro = Haro (1956BOTT....2n...8H) Arp = Arp (1966, Cat. <VII/74>) --- Note Individual note number=5 CG 3 = N2679/80 CG 21 = N2893 CG 33 = N3011 CG 61 = N3265 CG 118 = N3786 = Arp 294 CG 168 = N4253 --- James Marcout, Patricia Bauer CDS 1997 Sep 26 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_109_2376.xml Late-type stars in M31. I. Photometric study of AGB stars and metallicity gradients J/AJ/109/2480 J/AJ/109/2480 VI photometry of late-type stars in M31. I. Late-type stars in M31. I. Photometric study of AGB stars and metallicity gradients J P Brewer H B Richer D R Crabtree Astron. J. 109 2480 1995 1995AJ....109.2480B J/AJ/112/491 : Late-Type Stars in M31. II. (Brewer+ 1996) Photometry Stars, late-type We have imaged five 7'x7' fields in M31 spanning galactocentric radii from 4 to 32 kpc along the SW semi-major axis. The fields were observed through two broadband (V and I) and two narrowband (CN and TiO) ({DELTA}{nu}=+2.8100A and ({DELTA}{nu}=-1.7800A, respectively) filters. The broadband data were used to construct I, (V-I) color-magnitude diagrams (CMDs) and, in some of our fields, we found significant numbers of stars in the Cepheid instability strip. A distance modulus for the Cepheids in the middle field was found that agreed well with other values in the literature. The width of the giant branch (GB) in the I, (V-I) CMD of all five fields was investigated, and we show that in four of the fields a likely explanation for the GB width is a combination of both metallicity and mass variations. Using the broadband data, the asymptotic giant branch (AGB) luminosity functions (LFs) were measured in the five fields, and we show that differences exist between these LFs. We speculate on how the different star-forming histories in the fields may lead to the observed AGB LFs and GB widths. Using the narrowband data along with the broadband data we separated the AGB stars into carbon-rich (C) and oxygen-rich (M) types. The carbon stars LFs were used to obtain an estimate for the distance modulus of M31 which agrees with the value derived from Cepheids. The ratio of C- to M-stars (C/M) is believed to be an indicator of gaseous chemical abundance at the time of formation of these stars. We show that the C/M ratio increases smoothly with galactocentric distance, suggesting an inverse correlation with metallicity. This is the first demonstration of this effect within a single extragalactic system. We find that differences in the width of the GB and the AGB LFs do not significantly affect the C/M ratio. We consider the effect of the increasing C/M ratio on the ISM in M31, and cite evidence in favor of a model where the grain composition in M31 is a function of galactocentric distance.
Serendipity Field Field in which star/cluster was identified --- Xpos X coordinate on the I-band image pix Ypos Y coordinate on the I-band image pix Type Type of star/cluster number=1 OC: Open cluster; GC: Globular cluster; GSC: Star from HST Guide Star Catalog; Ceph: Cepheid variable; Irreg: Irregular variable; Eclip: Eclipsing variable; Short: Short period variable --- ID Identification from the literature --- Ref Reference code for ID number=2 1 Hodge 1981, Atlas of the Andromeda Galaxy (University of Washington Press, Seattle) 2 Hubble Space Telescope Guide Star Catalog 3 Baade & Swope (1965AJ.....70..212B) --- Coordinates and photometry of candidate C stars Coordinates and photometry of candidate M stars ID ID for each star, ordered by magnitude --- Xpos X coordinate on the I-band image pix Ypos Y coordinate on the I-band image pix Imag I magnitude mag e_Imag ALLSTAR error in Imag mag V-I V-I color mag e_V-I Error in V-I number=1 Error derived by adding ALLSTAR errors in quadrature. mag CN-TiO CB-TiO color mag e_CN-TiO Error in CN-TiO number=1 Error derived by adding ALLSTAR errors in quadrature. mag table2.tex AASTeX version of table2.dat table7.tex AASTeX version of table7.dat table8.tex AASTeX version of table8.dat field1.fit Field 1 I-band image, RA=0:41:41, DE=+40:59:00 field2.fit Field 2 I-band image, RA=0:41:08, DE=+40:50:41 field3.fit Field 3 I-band image, RA=0:40:22, DE=+40:36:24 field4.fit Field 4 I-band image, RA=0:39:24, DE=+40:14:32 field5.fit Field 5 I-band image, RA=0:35:42, DE=+39:29:03 CDS 1996 Jan 09 AAS CD-ROM series, Vol. 5, 1995 Lee Brotzman [ADS] 26-Sep-1995 J_AJ_109_2480.xml Embedded clusters in giant extragalactic H II regions. II. Evolutionary population synthesis model J/AJ/109/2503 J/AJ/109/2503 Synthesis model in HII regions. II. Embedded clusters in giant extragalactic H II regions. II. Evolutionary population synthesis model Y D Mayya Astron. J. 109 2503 1995 1995AJ....109.2503M H II regions Models, evolutionary Tables 3, 4, and 5 are given. Each table has been split into three parts, a, b, and c, where each part includes derived quantities for Initial Mass Functions (IMF) defined by slope, lower cutoff (M_l_), and upper cutoff (M_u_), as follows: part a: slope = 2.5, M_l_ = 1, M_u_ = 60 part b: slope = 3.5, M_l_ = 1, M_u_ = 30 part c: slope = 1.0, M_l_ = 1, M_u_ = 120 Tabulated quantities are smoothed over a period of 0.5Myr to suppress the short term fluctuations on the computer quantities. For the continuous star-formation model, constant star-formation rate (SFR) is assumed in computations of the tabulated quantities. Table 5 give the ages of the young and old bursts for the two-burst models. A stellar population synthesis model, suitable for comparison with Giant Extragalactic H II Regions (GEHRs), is constructed incorporating the recent developments in modeling stellar evolution by Maeder and co-workers and stellar atmospheres by Kurucz. A number of quantities suitable for comparison with broadband data of GEHRs in visible and near-infrared parts of the spectrum are synthesized in addition to the hydrogen and helium ionizing photon production rates at solar metallicities, for three scenarios of star formation - (i) instantaneous burst (IB); (ii) continuous star formation (CSF); and (iii) two bursts of star formation, with the older burst rich in red supergiants. For the IB case, evolution of color indexes shows three distinct phases - an initial steady blue phase, followed by a red bump (5-15Myr) and another steady phase with color indexes intermediate to the earlier two phases. CSF color indexes asymptotically reach peak values at ~10Myr, never reaching the reddest IB color indexes. Ionizing photon production rate falls off by an order of magnitude in 6Myr for IB, whereas it almost remains constant for the CSF model. Two-burst models with burst separations ~10Myr have properties of both IB and CSF, simultaneously producing the red IB color indexes and high ionizing photon rate, making such regions easily distinguishable using optical observations. Flat IMFs result in bluest color indexes when the massive stars are on the main sequence and reddest color indexes during the red supergiant phase of the evolving massive stars. Errors on the computed quantities due to the statistical uncertainties inherent in the process of star formation become negligible for cluster masses in excess of 10^5 M_{sun}_. Our GEHR spectra in the range 200nm to 3um are found to be in good agreement with the computations of Mas-Hesse & Kunth (1991A&AS...88..399M)
Derived quantities for star clusters with IB Derived quantities for star clusters with IB Derived quantities for star clusters with IB Derived quantities for star clusters with CSF Derived quantities for star clusters with CSF Derived quantities for star clusters with CSF Age Age of the cluster Myr M/L Ratio of total mass to bolometric lum. solMass/solLum M/Lv Ratio of total mass to visual luminosity solMass/solLum NLy Lyman continuum photon production rate per unit mass of the cluster ph/s/solMass fHe Fraction of hydrogen ionizing photons which are capable of ionizing helium --- Phi/Lb Ratio of expected Hbeta to blue band luminosity number=1 Lyman continuum photon rate N_L_ is also expressed in units or expected Hbeta luminosity {phi} from a nebula at 10,000K, and defined as: {phi}=4.78x10^-13^N_L_. {phi} in this equation has dimensions or erg/s/M_{sun}_, and N_L_ in ph/s/M_{sun}_. --- B-V B-V color index mag V-R V-R color index mag V-I V-I color index mag J-H J-H color index mag H-K H-K color index mag V-K V-K color index mag WHb Hbeta equivalent width number=2 Equivalent widths assuming a gas temperature of 10,000K. 0.1nm WHa Halpha equivalent width number=2 Equivalent widths assuming a gas temperature of 10,000K. 0.1nm Der. quantities for star clusters w/ two bursts Der. quantities for star clusters w/ two bursts Der. quantities for star clusters w/ two bursts T(yng) Age of the younger burst Myr T(old) Age of the older burst Myr M/L Ratio of total mass to bolometric lum. solMass/solLum M/Lv Ratio of total mass to visual luminosity solMass/solLum NLy Lyman continuum photon production rate per unit mass of the cluster ph/s/solMass fHe Fraction of hydrogen ionizing photons which are capable of ionizing helium --- Phi/Lb Ratio of expected Hbeta to blue band lum.(1) --- B-V B-V color index mag V-R V-R color index mag V-I V-I color index mag J-H J-H color index mag H-K H-K color index mag V-K V-K color index mag WHb Hbeta emission line equivalent width number=2 Equivalent widths assuming a gas temperature of 10,000K. 0.1nm WHa Halpha emission line equivalent width number=2 Equivalent widths assuming a gas temperature of 10,000K. 0.1nm CDS 1996 Jan 09 AAS CD-ROM series, Vol. 5, 1995 Lee Brotzman [ADS] 19-Jul-1995 J_AJ_109_2503.xml BVI CCD Photometry of NGC 5053: The Most Metal-Poor Galactic Globular Cluster J/AJ/109/269 J/AJ/109/269 Photometry of NGC 5053 BVI CCD Photometry of NGC 5053: The Most Metal-Poor Galactic Globular Cluster A Sarajedini A A E Milone Astron. J. 109 269 1995 1995AJ....109..269S Clusters, globular Photometry (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams are presented for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system.
NGC 5053 photometry Star Star number --- Xpos X pixel position pix Ypos Y pixel position pix Vmag V magnitude mag B-V B-V color mag V-I V-I color mag o_B-V Number of frame pairs on which each B-V measurement was made --- o_V-I Number of frame pairs on which each V-I measurement was made --- CDS 1995 Jul 10 AAS CD-ROM series, Vol. 4, 1995 Lee Brotzman [ADS] 29-Apr-1995 J_AJ_109_269.xml Ca II H and K filter photometry on the uvby system. II. The catalog of observations. J/AJ/109/2828 J/AJ/109/2828 CaII H and K filter photometry II. Ca II H and K filter photometry on the uvby system. II. The catalog of observations. B A Twarog B J Anthony-Twarog Astron. J. 109 2828 1995 1995AJ....109.2828T J/A+AS/102/89 : Olsen's Stroemgren photometry of G5-type HD stars Photometry, hk A catalog of 1990 stars on the Caby system is presented. The sample includes stars covering an extensive range in spectral type, luminosity class, and metallicity, as well as apparent magnitude. The hk indices are on the standard system defined in Anthony-Twarog et al. (1991AJ....101.1902A), while the V and (b-y) indices have been transformed to the system of Olsen (1993A&AS..102...89O), superseding the values in the original catalog of standard stars. Photometric system: Definition and properties of the H&K photometric system may be found at URL <http://obswww.unige.ch/gcpd/ph81.html>
The observations (Table 2 of the paper) HD Hentry Draper Catalogue designation --- Name1 Alternative designation number=1 alternative designations are in the following order of priority: Durchmusterung (BD, CD, CP); C Beers (1992AJ....103.1987B), or G from Giclas, Catalog <I/79> HR from Bright Star Catalog <V/50> LTT Luyten Two Tenths Catalogues, 1957, 1961 Anthony-Twarog & Twarog (1994AJ....107.1577A) RA Rose & Agostinho (1991AJ....101..950R) W Wilson 1953, Catalog <III/21> YC Jenkins, 1952, 1953, Yale Catalogue of Trigonometric Parallaxes, Catalog <I/81> --- Name2 Alternative designation number=1 alternative designations are in the following order of priority: Durchmusterung (BD, CD, CP); C Beers (1992AJ....103.1987B), or G from Giclas, Catalog <I/79> HR from Bright Star Catalog <V/50> LTT Luyten Two Tenths Catalogues, 1957, 1961 Anthony-Twarog & Twarog (1994AJ....107.1577A) RA Rose & Agostinho (1991AJ....101..950R) W Wilson 1953, Catalog <III/21> YC Jenkins, 1952, 1953, Yale Catalogue of Trigonometric Parallaxes, Catalog <I/81> --- Vmag Magnitude in V system mag e_Vmag Mean error on Vmag mag b-y colour index in Stroemgren system mag e_b-y Mean error on b-y mag hk index in Caby system mag e_hk standard deviation for a single observation mag Nobs Number of observations --- Class Classification of the star number=2 the classification is as follows: D for dwarfs redder than (b-y) = 0.41 G for giants cooler than (b-y) = 0.41 C for carbon stars Stars hotter than (b-y) = 0.41 have no classification. --- Francois Ochsenbein CDS 1995 Nov 21 Barbara Anthony-Twarog <ANTHONY@kustar.phsx.ukans.edu> J_AJ_109_2828.xml Observations and Analysis of the Contact Binary H235 in the Open Cluster NGC 752 J/AJ/109/359 J/AJ/109/359 H235 in NGC 752 Observations and Analysis of the Contact Binary H235 in the Open Cluster NGC 752 E F Milone C R Stagg B A Sugars J R McVean S J Schiller D H Kallrath J Bradstreet Astron. J. 109 359 1995 1995AJ....109..359M Clusters, open Stars, variable The short-period variable star Heinemann 235 in the open cluster NGC 752 has been identified as a contact binary with a variable period of about 0.4118 d. BVRI light curves and radial velocity curves have been obtained.
Photoelectric light curve data HJD Heliocentric Julian Date d Ph1 Phase of minima from ephemeris 1 Phase of minima calculated using ephemeris (1) from printed paper: E0 = 2 447 815.338(3), P = 0.411 83(12)d --- Ph3 Phase of minima from ephemeris 3 Phase of minima calculated using ephemeris (3) from printed paper: E0 = 2 446 785.8660(23), P = 0.411 775 0(10)d --- dVmag Differential V magnitude mag dBmag Differential B magnitude mag dRmag Differential R magnitude mag dImag Differential I magnitude mag d(B-V) Differential (B-V) color mag d(V-R) Differential (V-R) color mag d(V-I) Differential (V-I) color mag CDS 1995 Jul 10 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 29-Apr-1995 HJD completed at CDS) J_AJ_109_359.xml Integrated photoelectric magnitudes and color indices of bright galaxies in the Johnson UBV system. J/AJ/109/517 J/AJ/109/517 Photoelectric types of bright galaxies Integrated photoelectric magnitudes and color indices of bright galaxies in the Johnson UBV system. R Buta H G Corwin Jr. G de Vaucouleurs A de Vaucouleurs G Longo Astron. J. 109 517 1995 1995AJ....109..517B VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991) Galaxies, photometry Photometry, classification The photoelectric total magnitudes and color indices published in the Third Reference Catalogue of Bright Galaxies (RC3, Cat. <VII/155>) are based on an analysis of ~26000 B, 25000 B-V, and 17000 U-B multiaperture measurements available up to mid 1987 from nearly 350 sources. This paper provides the full details of the analysis and estimates of internal and external errors in the parameters. The derivation of the parameters is based on techniques described by de Vaucouleurs & Corwin (1977ApJS...33..219D) whereby photoelectric multiaperture data are fitted by mean Hubble-type-dependent curves which describe the integral of the B-band flux and the typical B-V and U-B integrated color gradients. A sophisticated analysis of the residuals of these measurements from the curves was made to allow for the random and systematic errors that affect such data. The result is a homogeneous set of total magnitudes B^A^_T_, total colors (B-V)_T_ and (U-B)_T_, and effective colors (B-V)_e_ and (U-B)_e_ for more than 3000 bright galaxies in RC3.
Photometric types Name Galaxy name as in RC3 (Cat. <VII/155>) --- Tc Catalogue type --- u_Tc Uncertainty flag on Tc --- Tp Photometric type --- James Marcout, Patricia Bauer CDS 1997 Jun 13 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_109_517.xml Total and Effective Colors of 501 Galaxies in the Cousins VRI Photometric System J/AJ/109/543 J/AJ/109/543 Color of Bright Galaxies Total and Effective Colors of 501 Galaxies in the Cousins VRI Photometric System R Buta K L Williams Astron. J. 109 543 1995 1995AJ....109..543B Galaxies Photometry Total color indices (V-R)tot, (V-I)tot and effective color indices (V-R)eff, (V-I)eff in the Cousins VRI photometric system are presented for 501 mostly normal galaxies. The colors are computed using a procedure outlined in the Third Reference Catalogue of Bright Galaxies (RC3) whereby standard color curves approximated by Laplace-Gauss integrals are fitted to observed photoelectric multiaperture photometry. 11 sources of such photometry were used, each source being assigned an appropriate weight according to a rigorous analysis of residuals of the data from the best-fitting standard color curves. Together with the integrated B-V and U-B colors provided in RC3, the analysis widens the range of wavelength of homogeneously defined colors of normal galaxies of all Hubble types. Color-color and color-type relations that can be modeled to understand the star formation history of galaxies are intrinsic in these data.
Total and effective V-R and V-I color indices for 501 galaxies Object Object name in various catalogues --- RC3 Numerical stage index in revised Hubble system, from the RC3 --- o_V-Rtot Number of observations of V-R --- V-Rtot Total V-R color index mag e_V-Rtot V-Rtot internal mean error mag V-Itot Total V-I color index mag e_V-Itot V-Itot internal mean error mag V-Reff Effective V-R color index mag e_V-Reff V-Reff internal mean error mag V-Ieff Effective V-I color index mag e_V-Ieff V-Ieff internal mean error mag TSSC_B-V Type index of B-V used to fit V-R The type index of the B-V standard color curve used to fit V-R (see Figure 6 of the Second Reference Catalogue of Bright Galaxies, RC2); T(SCC)= 20 refers to a curve of zero integrated color gradient. --- TSSC_U-B Type index of U-B used to fit V-I The type index of the U-B standard color curve used to fit V-I (see Figure 6 of RC2); T(SCC)= 20 refers to a curve of zero integrated color gradient. --- CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 29-Apr-1995 J_AJ_109_543.xml B,V Photometry of the RR Lyrae Stars in the Very Metal-Poor Globular Cluster NGC 5053 J/AJ/109/618 J/AJ/109/618 RR Lyrae Stars in NGC 5053 B,V Photometry of the RR Lyrae Stars in the Very Metal-Poor Globular Cluster NGC 5053 J M Nemec M Mateo J M Schombert Astron. J. 109 618 1995 1995AJ....109..618N Clusters, globular Stars, metal-deficient Stars, variable Individual measurements of B and V are presented for ten RR Lyrae stars in NGC 5053 derived from CCD frames taken on 15 nights between 1985 and 1994. Estimates of fundamental photometric parameters are presented for the ten stars, including mean B and V magnitudes, pulsation periods, pulsation amplitudes, <B>-<V> colors, and period change rates.
Photometry of the ab-type RR Lyrae star V1 Photometry of the c-type RR Lyrae star V2 Photometry of the ab-type RR Lyrae star V3 Photometry of the ab-type RR Lyrae star V4 Photometry of the ab-type RR Lyrae star V5 Photometry of the c-type RR Lyrae star V6 Photometry of the c-type RR Lyrae star V7 Photometry of the c-type RR Lyrae star V8 Photometry of the ab-type RR Lyrae star V9 Photometry of the c-type RR Lyrae star V10 Night Observing night number --- HJD HJD of midpoint of observation The mid-HJD of each exposure was computed using M. Fletcher's (Dominion Astrophysical Observatory) REDSUN program. d Vmag V magnitude mag e_Vmag Uncertainty in Vmag The uncertainties are lower limits since they are the quantities returned by the photometry programs and do not include the systematic zero-point uncertainties introduced by the transformation from instrumental to standard magnitudes. mag Bmag B magnitude In file table3.dat, night 17, HJD 8416.7570, the B magnitude was derived from I through a V-I,B-V transformation. mag e_Bmag Uncertainty in Bmag mag Properties of the RR Lyrae stars in NGC 5053 Star Star number, V1 to V10 --- l_P In one case, V10, this is '>=' --- P Pulsation period for the current epoch d Beta Period rate change = delta P / delta t 10-9 Type Bailey type --- Bmin B magnitude at minimum light mag e_Bmin Uncertainty in Bmin Uncertainties in minimum and maximum magnitudes are subjective estimates based on the number and quality of the observations. mag Bmax B magnitude at maximum light mag e_Bmax Uncertainty in Bmax mag AB B amplitude mag e_AB Uncertainty in AB, based on e_Bmin,e_Bmax mag Vmin V magnitude at minimum light mag e_Vmin Uncertainty in Vmin mag Vmax V magnitude at maximum light mag e_Vmax Uncertainty in Vmax mag AV V amplitude mag e_AV Uncertainty in AV, based on e_Vmin,e_Vmax mag <B> Intensity mean <B> magnitude mag e_<B> Uncertainty in <B> mag <V> Intensity mean <V> magnitude mag e_<V> Uncertainty in <V> mag <B>-<V> Intensity mean <B>-<V> color mag e_<B>-<V> Uncertainty in <B>-<V> mag table1.tex TeX (plain) version of Table 1 table2.tex TeX (plain) version of Table 2 table3.tex TeX (plain) version of Table 3 table4.tex TeX (plain) version of Table 4 table5.tex TeX (plain) version of Table 5 table6.tex TeX (plain) version of Table 6 table7.tex TeX (plain) version of Table 7 table8.tex TeX (plain) version of Table 8 table9.tex TeX (plain) version of Table 9 table10.tex TeX (plain) version of Table 10 table11.tex TeX (plain) version of Table 11 CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 02-May-1995 (JD completed at CDS) J_AJ_109_618.xml HST Observations of the Core of the Globular Cluster NGC 6624 J/AJ/109/639 J/AJ/109/639 The Core of NGC 6624 HST Observations of the Core of the Globular Cluster NGC 6624 C Sosin I R King Astron. J. 109 639 1995 1995AJ....109..639S Clusters, globular Photometry Positional data The Faint Object Camera on the Hubble Space Telescope (HST) has been used to observe three fields near the center of the post-collapse globular cluster NGC 6624 in B and V. Individual stellar positions and a maximum-likelihood technique were used to measure a position for the cluster center. These positions and the position of the x-ray source 4U 1820-30 were then transferred to right ascension and declination, and an error of 1.8" in an earlier paper was corrected. Photometry is provided down to the main-sequence turnoff near the cluster center, and more than three magnitudes below the turnoff in the outermost field at r=28".
Photometry of all stars brighter than V = 20 in our inner two fields in NGC 6624 ID Identification number --- Field Field number 1=central 11x11 arcsec image, 2=image at r=10" --- Xpos X coordinate on F480LP image under Field pix Ypos Y coordinate on F480LP image under Field pix oRA RA (J2000) relative to cluster center Coordinates of cluster center: B1950 RA 18h 20m 27.686s +/- 0.021s Dec -30d 23' 17.10" +/- 0.27" J2000 RA 18h 23m 40.453s +/- 0.021s Dec -30d 21' 40.75" +/- 0.27" arcsec oDE Dec (J2000) relative to cluster center arcsec m480 F480LP instrumental magnitude mag m430-m480 F430W - F480LP color (HST instr. system) mag Vmag V magnitude mag B-V B-V color mag Comment Comments --- Photometry of all stars brighter than V = 23 in our outermost FOC field in NGC 6624 ID Identification number --- Xpos X coord. on outermost (r=28") F480LP image pix Ypos Y coord. on outermost (r=28") F480LP image pix oRA RA (J2000) relative to star at (257,286) Coordinates of bright star at (257,286) in outermost field: B1950 RA 18h 20m 29.141s +/- 0.012s Dec -30d 22' 54.91" +/- 0.15" J2000 RA 18h 23m 41.898s +/- 0.012s Dec -30d 21' 18.45" +/- 0.15" arcsec oDE Dec (J2000) relative to star at (257,286) arcsec m480 F480LP instrumental magnitude mag m430-m480 F430W - F480LP color (HST instr. system) mag Vmag V magnitude mag B-V B-V color mag CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 25-Apr-1995 J_AJ_109_639.xml Young Globular Clusters in the Milky Way: Arp 2 J/AJ/109/650 J/AJ/109/650 Arp 2 Young Globular Clusters in the Milky Way: Arp 2 R Buonanno C E Corsi F Fusi Pecci H B Richer G G Fahlman Astron. J. 109 650 1995 1995AJ....109..650B Clusters, globular Photometry, CCD We have obtained the first B,V CCD color-magnitude diagram (CMD) of the galactic globular cluster Arp 2. About 1600 stars have been measured between the tip of the red giant branch at V ~ 15.5 and V ~ 23.5, about two magnitudes below the main sequence turnoff. A centrally concentrated population of blue stragglers has been detected. The slope of the red giant branch and the overall CMD morphology are consistent with that of a metal-poor cluster, with [Fe/H] = 18.4 +/- 0.25. A preliminary spectroscopic measurement based on the Ca II triplet yields [Fe/H] = -1.73 +/- 0.05. The comparison of the CMD of Arp 2 with that of other clusters favors a value more metal-poor than that indicated by the Ca II triplet. In this respect, Arp 2 is similar to Ruprecht 106 [Buonanno et al. AJ, 100, 1811 (1990), AJ, 105, 184 (1993)]. Differential ages between Arp 2 and a number of reference clusters are obtained from the vertical age parameter Delta V^TO_HB, and the horizontal age parameter, Delta (B-V)^TO_RGB. By requiring both age estimators to give consistent results, we find that Arp 2 is ~3 Gyr younger than the group of the metal-poor clusters and slightly older than Ruprecht 106. The detection of young metal-poor clusters ([Fe/H] <= -1.8) implies a complex scenario for the origin of the galactic halo, possibly involving interactions with satellite galaxies and their cluster systems.
Magnitudes, colors, and positions of stars in the central field of Arp 2 Star Star number --- Vmag V magnitude mag B-V (B-V) color mag Xpos X coordinate in local system X and Y coordinates in local system (hence, useful just for identification purposes) and are expressed in arcseconds relative to an arbitrary "center" adopted for the cluster. arcsec Ypos Y coordinate in local system arcsec table2.tex TeX version of Table 2 CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 26-Apr-1995 J_AJ_109_650.xml A 2.2um imaging survey of the Orion A molecular cloud J/AJ/109/709 J/AJ/109/709 K survey of Ori A molecular cloud A 2.2um imaging survey of the Orion A molecular cloud B Ali D L Depoy Astron. J. 109 709 1995 1995AJ....109..709A Infrared sources Photometry, infrared Positional data We present results from a 2.2um (limiting K about 14.5mag) survey of the northern portion of the Orion A molecular cloud. A total of 3548 sources were detected in the 1472arcmin^2^ area surveyed. We detect clustering of 2.2um sources at the locations of the Trapezium and OMC-2. No strict boundaries for these clusters could be drawn from our data because we find that the entire region surveyed shows an overabundance of sources when compared with background field levels. We find that the form of the observed K luminosity function (KLF) of stars near the Trapezium is consistent with that predicted from a Miller and Scalo (ApJS 41, 513 (1979) IMF, if the age of the cluster is about 1Myr. Away from the Trapezium and the OMC-2, the KLF of stars suggests that either this population contains more low mass stars or that it is older than the Trapezium stars. The survey was carried out using the Ohio State InfraRed Imaging System (OSIRIS) 256x256 HgCdTe array on the Perkins 1.8m telescope in November 1992. In survey mode OSIRIS provides a spatial resolution of 1.50arcsec/pixel; the total field of view of the camera is 6.4arcmin. The telescope was rastered on 4.2arcmin steps to produce a mosaic approximately 39x39arcmin, centered near the Trapezium. A total of 81 K-band images were obtained, each with an exposure time about 3s.
*List of the 3548 sources Seq Designation [AD95] --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Kmag K magnitude (2.2um) mag e_Kmag Mean error on Kmag mag Francois Ochsenbein CDS 1995 Oct 02 Babar Ali <ali@payne.mps.ohio-state.edu> J_AJ_109_709.xml The Enigmatic WN8 Stars: Intensive Photometry of Four Southern Stars on Time Scales From 30 min to 3 Months J/AJ/109/817 J/AJ/109/817 Photometry of WN8 Stars The Enigmatic WN8 Stars: Intensive Photometry of Four Southern Stars on Time Scales From 30 min to 3 Months I Antokhin J -F Bertrand R Lamontagne A F J Moffat J Matthews Astron. J. 109 817 1995 1995AJ....109..817A Photometry Stars, Wolf-Rayet We present the first results of an extensive photometric study of the most intrinsically variable Wolf-Rayet stars: the WN8 subclass. Some 375 individual differential observations of WR16 and WR40 were obtained over a contiguous interval of ~3 months in a narrow visual continuum bandpass. Over the same interval, we obtained roughly 200 broadband V observations of the fainter WN8 stars WR66 and WR82. All four WN8 stars show significant random variability on time scales of hours to ~a day -- probably related to the stochastic formation, propagation, and decay of emitting/scattering inhomogeneities in the winds. Unlike for WR66 and WR82, the photometric behaviour of WR16 and WR40 is more deterministic with ~two possible periods in the range ~2-30 days -- possibly related to some kind of LBV, binary, or rotation phenomenon. In addition, WR82 shows a possible secular decline during the 3 months and WR66 reveals a clear periodicity of 3.51 h. This short period may be related to nonradial pulsations or a spiral-in binary process invoking a low-mass, compact companion as seen in the massive x-ray binary Cyg X-3, a WN7 + c system of period 4.8 h.
Comparison stars for the WN8 stars WR WR number --- Other Other name --- vmag v magnitude mag b-v b-v color mag Cmp Comparison star number (C1 or C2) --- Name Comparison star name --- Sp Spectral type --- Vmag V magnitude mag WR-C Difference between comparison and WR mag e_WR-C Error (sigma) in WR-C mag C2-C1 Difference between comparison star mag e_C2-C1 Error (sigma) in C2-C1 mag Narrowband visual photometry for WR16 Narrowband visual photometry for WR40 Broadband visual photometry for WR66 Broadband visual photometry for WR82 HJD Heliocentric Julian Date d WR-C1 WR-C1 differential magnitude mag WR-C2 WR-C2 differential magnitude mag C2-C1 C2-C1 differential magnitude mag table.tex LaTeX document to format tables 2, 3, 4, & 5 table2.tex AASTeX version of Table 2 table3.tex AASTeX version of Table 3 table4.tex AASTeX version of Table 4 table5.tex AASTeX version of Table 5 CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 26-Apr-1995 (JD completed at CDS) J_AJ_109_817.xml Kinematics and Dynamics of the MKW/AWM Poor Clusters J/AJ/109/874 J/AJ/109/874 Kinematics of MKW and AWM Poor Clusters Kinematics and Dynamics of the MKW/AWM Poor Clusters T C Beers J R Kriessler C M Bird J P Huchra Astron. J. 109 874 1995 1995AJ....109..874B VII/144 : The CfA redshift catalogue (Huchra et al., 1992)) Clusters, galaxy Redshifts We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 <= M/L_B(0) <= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.
*Velocities for galaxies in poor clusters Cluster MKW or AWM cluster number MKW is the list by Morgan, Kayser and White [1975ApJ...199..545M]; AWM is the list by Albert, White and Morgan [1977ApJ...211..309A] --- Galaxy Name of the galaxy If the galaxy name is blank the data in the remainder of the fields are continuations of the previous record. --- ID Galaxy identification number with sample This is the number of each galaxy within the sample followed by a subsample descriptor. Lower case letters a and b refer to redshifts which appear in two different subsamples according to: a Galaxies in common MKW 6 & MKW7/8 b Galaxies in common MKW 4s & AWM 2 --- RAh Right ascension 1950.0 h RAm R.A. min DE- Declination sign 1950.0 --- DEd Dec. deg DEm Dec. arcmin mB0 Apparent magnitude on Zwicky B0 scale mag RV Galaxy heliocentric radial velocity km/s e_RV Galaxy heliocentric radial velocity error km/s Source Source codes Codes given in Huchra et al. [1992BICDS..41...31H] or: -4 Bothun 1991, private communication -4-1 Mould 1991, private communication -4-2 Mould et al. 1991, private communication -5-2 Strauss et al. 1994, private communication --- CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 03-May-1995 J_AJ_109_874.xml Hubble Space Telescope observations of young star clusters in NGC 4038/4039, "The Antennae" galaxies J/AJ/109/960 J/AJ/109/960 Young star clusters in The Antennae Hubble Space Telescope observations of young star clusters in NGC 4038/4039, "The Antennae" galaxies B C Whitmore F Schweizer Astron. J. 109 960 1995 1995AJ....109..960W Associations, stellar Photometry New high-resolution images of the disks of NGC 4038/4039 obtained with the Wide Field Camera of the Hubble Space Telescope (HST) are presented. NGC 4038/4039, nicknamed "The Antennae," is a prototypical example of a pair of colliding galaxies believed to be at an early stage of a merger. Down to the limiting magnitude of V~23mag, the HST images reveal a population of over 700 blue pointlike objects within the disks. The mean absolute magnitude of these objects is M_V_=-11mag, with the brightest objects reaching M_V_~-15. Their mean apparent color indices are U-V=-0.7mag and V-I=0.8mag on the Johnson UVI passband system, while their mean indices corrected for internal reddening are (U-V)_0_=-1.0mag and (V-I)_0_=0.5. Their mean effective radius, determined from slightly resolved images, is 18pc (for H0=50km/s/Mpc). Based on their luminosities and resolution, most of these objects cannot be individual stars, but are likely young compact star clusters. The brighter ones are similar to the objects found in NGC 1275 and NGC 7252, which appear to be young globular clusters formed during recent galaxy mergers. Based on their U-V and V-I colors, the brightest, bluest clusters of NGC 4038/4039 appear to be less than 10Myr old. Most of these bright clusters are relatively tightly clustered themselves, with typically a dozen individual clusters belonging to a complex identified as a giant H II region from ground-based observations. The cluster luminosity function (LF) is approximately a power law, {Phi}(L)dL is proportional to L^(-1.78+/-0.05)^dL, with no hint of a turnover at fainter magnitudes. This power-law shape agrees with the LF of Magellanic Cloud clusters and Galactic open clusters, but differs from the LF of old globular cluster systems that is typically Gaussian with a FWHM of ~3mag. Possible explanations for this apparent difference include: (1) We have not observed faint enough to see the turnover, (2) the initial LF of star clusters is a power law but the fainter objects dissolve with time, (3) conditions at the present epoch favor the formation of a wide range of cluster masses while conditions at earlier epochs favored the formation of massive clusters, and (4) the NGC 4038/4039 clusters may not evolve into normal globular clusters. Besides the blue clusters, we also find about a dozen extremely red objects with V-I>3.0. The highest number density of these red objects is found in the SE quadrant, where star formation appears to be most recent. We propose that these objects may be very young star clusters still embedded in their placental dust cocoons.
HST
Positions, magnitudes, and sizes of the pointlike objects in NGC 4038/4039 Obj Object number --- Note Table note reference letter a) Very red object. In this case, the V-I and e_V-I fields are instead Johnson I magnitudes and errors respectively. Also the U-V and e_U-V fields are actually V-I colors and error, respectively. b) Nucleus of NGC 4039 c) Evaluated as if a star cluster. However, this is almost certainly a normal galactic nucleus, hence the magnitude and radius are misleading since the object is very extended. d) Probably a star, since Reff is <-10pc (i.e., below the cutoff), and the I image shows possible tendrils which are characteristic of a point source. --- oRA RA offset from object #442 Offset in RA and DEC from object # 442 at a position RA=12h01m52.891s, DEC=-18deg52'09.49" (J2000 coordinates in the coordinate frame of the Guide Star Catalog) arcsec oDE Dec offset from object #442 arcsec Vmag Johnson V magnitude mag e_Vmag Uncertainty in Vmag mag V-I Johnson V-I color If Note field contains letter 'a', these fields are actually the Johnson I magnitude, error in I magnitude, V-I color and error in V-I color, respectively. mag e_V-I Uncertainty in V-I mag U-V Johnson U-V color mag e_U-V Uncertainty in U-V mag Reff Effective radius of the object pc CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 03-May-1995 J_AJ_109_960.xml The luminosity function of elliptical galaxies J/AJ/110/1032 J/AJ/110/1032 APM elliptical galaxies radial velocities The luminosity function of elliptical galaxies H Muriel M A Nicotra D G Lambas Astron. J. 110 1032 1995 1995AJ....110.1032M J/MNRAS/278/1025 : The APM Bright Galaxy Catalogue (Loveday 1996) Galaxies, photometry Radial velocities We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.
New radial velocities of APM Bright Galaxies Survey (APMBGS) ellipticals RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec bJmag bJ magnitude mag RV Radial velocity km/s James Marcout, Patricia Bauer CDS 1997 Apr 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_110_1032.xml Photoelectric photometry of Zwicky Galaxies J/AJ/110/1083 J/AJ/110/1083 Photometry of Zwicky Galaxies Photoelectric photometry of Zwicky Galaxies M Takamiya R G Kron G E Kron Astron. J. 110 1083 1995 1995AJ....110.1083T Galaxies, photometry Multiaperture photoelectric measurements in the B and V bands are presented for 601 galaxies in Volumes I, II, and V of Zwicky's catalogue. Large aperture observations were made in the 1960's with the Lick 3 m telescope and the USNO 1 m telescope. Systematics in Zwicky's magnitude system are investigated as a function of magnitude and direction in the sky. The photoelectric sample is argued to be representative of galaxies in Zwicky's catalogue at B ~ 15. A strong systematic error in Zwicky's magnitudes is apparent in Volume I fainter than m_z = 15.0. The B-V color distribution is discussed.
The photoelectric data RAh Right ascension 1950 from CGCG <VII/4> h RAm Right ascension 1950 from CGCG min DE- Declination sign from CGCG --- DEd Declination 1950 from CGCG deg DEm Declination 1950 from CGCG arcmin mz Magnitude listed in CGCG <VII/4> mag Name NGC, IC or UGC number --- Vmag V magnitude measured within aperture radius mag n_Vmag Note flags for Vmag number=1 Note flags for V and B magnitudes: a Data marked with "x" in original data sheets b Data marked with "?" in original data sheets c Missing computer log entry d Perhaps 1/2 mag shunt error e |mag - mag_{rc3}| > 0.75 --- Bmag B magnitude measured within aperture radius mag n_Bmag Note flags for Bmag number=1 Note flags for V and B magnitudes: a Data marked with "x" in original data sheets b Data marked with "?" in original data sheets c Missing computer log entry d Perhaps 1/2 mag shunt error e |mag - mag_{rc3}| > 0.75 --- B-V B-V color mag Delta_m Aperture correction mag Rad Aperture radius arcsec Date Date of observation "DD/MM/YY" table1.tex AASTeX version of table1.dat CDS 1996 Aug 23 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 27-Sep-1995 UNKNOWN UNKNOWN The Date originally in MM/DD/YY has been converted to FITS standard, and the fields originally blank (RA, DE, Name, Date) for continuation have been filled. J_AJ_110_1083.xml The optical gravitational lensing experiment: variable stars in the Sagittarius dwarf spheroidal galaxy J/AJ/110/1141 J/AJ/110/1141 Variables in the Sagittarius dSph The optical gravitational lensing experiment: variable stars in the Sagittarius dwarf spheroidal galaxy M Mateo M Kubiak M Szymanski J Kaluzny W Krzeminski A Udalski Astron. J. 110 1141 1995 1995AJ....110.1141M Gravitational lensing Photometry, CCD Stars, variable We present time-series CCD photometry of a field in the newly discovered dwarf spheroidal galaxy in Sagittarius (hereafter Sgr), and of a nearby control field. These data, which consist of VI images obtained during the 1994 OGLE season, were used to identify and study variable stars in both fields. We discovered ten variable stars in the Sgr field, nine of which have light curves and periods consistent with RR Lyr stars or anomalous Cepheids. The control field contains four short-period contact eclipsing binaries, but no pulsating variables. The variables in the Sgr field include a bright RR Lyr star that is almost certainly located in front of Sgr in the galactic bulge, a short-period contact binary located near or within Sgr, and a short-period pulsating star that may either be a foreground halo RR Lyr star or an anomalous Cepheid within Sgr. The seven remaining variables in the Sgr field are RR Lyr stars with very similar mean apparent magnitudes; we conclude that they are members of Sgr. We estimate the total number of RR Lyr stars in Sgr to be 1930+/-730 if M(V,Sgr)=-13, or 310+/-120 if M(V,Sgr)=-11. The frequency of pulsating variables in Sgr is consistent with earlier conclusions that the galaxy consists of a predominant old (age>~10Gyr) population.
Sgr field 19 06 11 -30 25 22 Control field 18 33 26 -40 57 57
V-band data for the Sgr-field variables HJD Heliocentric Julian Date --- VmagV1 Sgr V1 calibrated V magnitude mag e_VmagV1 VmagV1 error mag PhasV1 Sgr V1 phase --- VmagV2 Sgr V2 calibrated V magnitude mag e_VmagV2 VmagV2 error mag PhasV2 Sgr V2 phase --- VmagV3 Sgr V3 calibrated V magnitude mag e_VmagV3 VmagV3 error mag PhasV3 Sgr V3 phase --- VmagV4 Sgr V4 calibrated V magnitude mag e_VmagV4 VmagV4 error mag PhasV4 Sgr V4 phase --- VmagV5 Sgr V5 calibrated V magnitude mag e_VmagV5 VmagV5 error mag PhasV5 Sgr V5 phase --- VmagV6 Sgr V6 calibrated V magnitude mag e_VmagV6 VmagV6 error mag PhasV6 Sgr V6 phase --- VmagV7 Sgr V7 calibrated V magnitude mag e_VmagV7 VmagV7 error mag PhasV7 Sgr V7 phase --- VmagV8 Sgr V8 calibrated V magnitude mag e_VmagV8 VmagV8 error mag PhasV8 Sgr V8 phase --- VmagV9 Sgr V9 calibrated V magnitude mag e_VmagV9 VmagV9 error mag PhasV9 Sgr V9 phase --- VmagV10 Sgr V10 calibrated V magnitude mag e_VmagV10 VmagV10 error mag PhasV10 Sgr V10 phase --- V-band data for the Control-field variables HJD Heliocentric Julian Date --- VmagV1c Control V1 calibrated V magnitude mag e_VmagV1c VmagV1c error mag PhasV1c Control V1 phase --- VmagV2c Control V2 calibrated V magnitude mag e_VmagV2c VmagV2c error mag PhasV2c Control V2 phase --- VmagV3c Control V3 calibrated V magnitude mag e_VmagV3c VmagV3c error mag PhasV3c Control V3 phase --- VmagV4c Control V4 calibrated V magnitude mag e_VmagV4c VmagV4c error mag PhasV4c Control V4 phase --- I-band data for the Sgr-field variables HJD Heliocentric Julian Date --- ImagV1 Sgr V1 calibrated I magnitude mag e_ImagV1 ImagV1 error mag PhasV1 Sgr V1 phase --- ImagV2 Sgr V2 calibrated I magnitude mag e_ImagV2 ImagV2 error mag PhasV2 Sgr V2 phase --- ImagV3 Sgr V3 calibrated I magnitude mag e_ImagV3 ImagV3 error mag PhasV3 Sgr V3 phase --- ImagV4 Sgr V4 calibrated I magnitude mag e_ImagV4 ImagV4 error mag PhasV4 Sgr V4 phase --- ImagV5 Sgr V5 calibrated I magnitude mag e_ImagV5 ImagV5 error mag PhasV5 Sgr V5 phase --- ImagV6 Sgr V6 calibrated I magnitude mag e_ImagV6 ImagV6 error mag PhasV6 Sgr V6 phase --- ImagV7 Sgr V7 calibrated I magnitude mag e_ImagV7 ImagV7 error mag PhasV7 Sgr V7 phase --- ImagV8 Sgr V8 calibrated I magnitude mag e_ImagV8 ImagV8 error mag PhasV8 Sgr V8 phase --- ImagV9 Sgr V9 calibrated I magnitude mag e_ImagV9 ImagV9 error mag PhasV9 Sgr V9 phase --- ImagV10 Sgr V10 calibrated I magnitude mag e_ImagV10 ImagV10 error mag PhasV10 Sgr V10 phase --- I-band data for the Control-field variables HJD Heliocentric Julian Date --- ImagV1c Control V1 calibrated I magnitude mag e_ImagV1c ImagV1c error mag PhasV1c Control V1 phase --- ImagV2c Control V2 calibrated I magnitude mag e_ImagV2c ImagV2c error mag PhasV2c Control V2 phase --- ImagV3c Control V3 calibrated I magnitude mag e_ImagV3c ImagV3c error mag PhasV3c Control V3 phase --- ImagV4c Control V4 calibrated I magnitude mag e_ImagV4c ImagV4c error mag PhasV4c Control V4 phase --- CDS 1996 Jan 10 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 30-Oct-1995 J_AJ_110_1141.xml An X-ray survey of the open cluster NGC 6475 (M7) with ROSAT. J/AJ/110/1229 J/AJ/110/1229 ROSAT X-ray survey in NGC 6475 An X-ray survey of the open cluster NGC 6475 (M7) with ROSAT. C F Prosser J R Stauffer J -P Caillault S Balachandran R A Stern S Randich Astron. J. 110 1229 1995 1995AJ....110.1229P Clusters, open Photometry, CCD X-ray sources A ROSAT X-ray survey, with complementary optical photometry, of the open cluster NGC 6475 has enabled the detection of ~50 late-F to K0 and ~70 K/M dwarf new candidate members, providing the first reliable detection of low-mass stars in this low galactic latitude, 220Myr old cluster. The X-ray observations reported here have a typical limiting sensitivity of L_X_ ~ 10^29^erg/s. The detection frequency of early type cluster members is consistent with the hypothesis that the X-ray emitting early type stars are binary systems with an unseen, low-mass secondary producing the X-rays. The ratio between X-ray and bolometric luminosity among NGC 6475 members saturates at a spectral-type/color which is intermediate between that in much younger and in much older clusters, consistent with rotational spindown of solar-type stars upon their arrival on the ZAMS. The upper envelope of X-ray luminosity as a function of spectral type is comparable to that of the Pleiades, with the observed spread in X-ray luminosity among low-mass members being likely due to the presence of binaries and relatively rapid rotators. However, the list of X-ray selected candidate members is likely biased against low-mass, slowly rotating single stars. While some preliminary spectroscopic information is given in an appendix, further spectroscopic observations of the new candidate members will aid in interpreting the coronal activity among solar-type NGC 6475 members and their relation to similar stars in older and younger open clusters.
ROSAT NGC 6475 M 7 17 53.9 -34 49
X-ray source list X-ray source list: Weaker possible sources ID Identification number [PSC95] --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Off-axis Distance off-axis from the center of the PSPC field arcmin Exp Exposition time s CRate Count rate s-1 e_CRate rms uncertainty on CRate s-1 S/Nb Broadband (0.07-2.4keV) signal to noise ratio --- S/Nh Hardband (0.5-1.8keV) signal to noise ratio --- logLx X-ray luminosity [10-7W] l_HR Limit flag on HR --- HR Hardness ratio --- DRA Offset on right ascension between X-ray and optical positions arcsec DDE Offset on declination between X-ray and optical positions arcsec Vmag V magnitude mag B-V B-V colour index mag V-Ic V-Ic colour index mag Member Membership --- o_Vmag Number of observation in V band --- o_Bmag Number of observation in B band --- o_Icmag Number of observation in Ic band --- Name Optical counterpart name when available number=1 Koelbloed (1959BAN....14..265K) name when available, otherwise, a letter designation "A", "B", etc. is assigned. --- GSC GSC number --- Note Notes number=2 the following abbreviations are used: ?source: weak sources which have been considered questionable upon visual inspection of the data rib: sources which may be partially obscured by the PSPC support structure --- ESO CASPEC radial and rotational velocities (1994 April 21-25 UT) Star Star name --- Vmag V Magnitude mag B-V B-V colour index mag V-Ic V-Ic colour index mag RV Radial velocity km/s u_RV Uncertainty flag (:) on RV --- l_Vrot Limit flag on Vrot --- Vrot Rotational velocity km/s u_Vrot Uncertainty flag on Vrot --- Member Member --- HJD Heliocentric Julian date d Note Notes --- James Marcout, Patricia Bauer CDS 1997 Jun 13 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_110_1229.xml Periodic light curve changes for Beta Lyrae J/AJ/110/1350 J/AJ/110/1350 Beta Lyrae light curve changes Periodic light curve changes for Beta Lyrae W Van Hamme R E Wilson E F Guinan Astron. J. 110 1350 1995 1995AJ....110.1350V Photometry Stars, variable Tables 2-5 present the original observations made with the 38cm reflector at Villanova (VIL) and the 25cm automated photoelectric telescope (APT), located on Mount Hopkins, Arizona. All differential magnitudes are with respect to the comparison star Gam Lyr. The Halpha and Hbeta filters are broad, with full width at half maximum (FWHM) 29 and 18 nm, respectively. The effective wavelengths are 660 and 487 nm. The Balmer lines presumably have only minor influences on these rather wide bandpasses. We apply a variety of classical and recently developed periodicity analyses to light curves of Beta Lyrae in 9 eras that extend over a range of about 150 years. Some new data are tabulated. Most periodic variations that have been reported in the literature do not pass standard significance tests, according to our adopted criteria. Certain other periods do pass the tests, although most do so only for one, or at most two, data sets. Our main findings are that a period of about 9 months is present in all data sets and that it connects extremely well in phase from era to era, all the way back to Baxendell's observations of 1840-1877. The semiamplitude is small but reasonably consistent, averaging about 2% of the flux in the light curve maxima. Any substantially larger excursions that occur are nonperiodic. Phase coherence of the 9 month period is fairly good, even with a linear ephemeris, and becomes excellent if one allows for a slow sinusoidal variation of the 9 month periodicity. There is some evidence for a monotonic decrease in the amplitude of the 9 month periodicity with increasing wavelength.
alpha Lyr HD 172167 HR 7001 18 36 55.4 +38 46 47 beta Lyr HD 174638 HR 7106 18 50 04.7 +33 21 46
beta Lyrae Villanova Halpha (wide) observations beta Lyrae Villanova Hbeta (wide) observations beta Lyrae Villanova Stromgren y observations HJD1 Heliocentric Julian Date d dm Differential magnitude mag beta Lyrae APT observations HJD Heliocentric Julian Date d dVmag Differential V mag (Var. - Comp.) mag dRmag Differential R mag (Var. - Comp.) mag dImag Differential I mag (Var. - Comp.) mag dVc Differential V mag (Check - Comp.) mag dRc Differential R mag (Check - Comp.) mag dIc Differential I mag (Check - Comp.) mag CDS 1996 Jan 25 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 28-Sep-1995 J_AJ_110_1350.xml Planetary-induced nutation of the Earth: direct terms J/AJ/110/1420 J/AJ/110/1420 Nutation of the Earth Planetary-induced nutation of the Earth: direct terms J G Williams Astron. J. 110 1420 1995 1995AJ....110.1420W Earth Full caption for table 2: Direct planetary-induced nutations with amplitudes in longitude larger than 0.5 microarcsec. Each argument consists of a linear combination of the mean longitudes of the seven planets Mercury- Uranus, and the general precession p accumulated from J2000. The degree is the implicit power of the planetary eccentricities and inclinations. Small torques by the planets can alter the direction of the Earth's rotation axis in space. These direct planetary-induced nutations have been computed using a numerical technique. 62 nutation terms with periods between 0.2 and 883yr are presented. The maximum nutation is 0.5mas. Also given are planetary-induced rates and accelerations of precession and obliquity.
Direct planetary-induced nutations ArgQ Mercury mean longitude multiplier --- ArgV Venus mean longitude multiplier --- ArgE Earth mean longitude multiplier --- ArgM Mars mean longitude multiplier --- ArgJ Jupiter mean longitude multiplier --- ArgS Saturn mean longitude multiplier --- ArgU Uranus mean longitude multiplier --- JPR Precession multiplier from J2000 --- PsiSin Sine coefficient of nutation in longitude number= Integers which multiply the mean longitudes of the seven planets Mercury-Uranus in the argument. number= Integer multiplying precession accumulated from J2000 in the argument. uarcsec PsiCos Cosine coefficient of nutation in long. number= Integers which multiply the mean longitudes of the seven planets Mercury-Uranus in the argument. number= Integer multiplying precession accumulated from J2000 in the argument. uarcsec EpsSin Sine coefficient of nutation in obliquity number= Integers which multiply the mean longitudes of the seven planets Mercury-Uranus in the argument. number= Integer multiplying precession accumulated from J2000 in the argument. uarcsec EpsCos Cosine coefficient of nutation in obliq. number= Integers which multiply the mean longitudes of the seven planets Mercury-Uranus in the argument. number= Integer multiplying precession accumulated from J2000 in the argument. uarcsec Per Period in days number= Integers which multiply the mean longitudes of the seven planets Mercury-Uranus in the argument. number= Integer multiplying precession accumulated from J2000 in the argument. d PerJY Period in Julian years number= Integers which multiply the mean longitudes of the seven planets Mercury-Uranus in the argument. number= Integer multiplying precession accumulated from J2000 in the argument. yr Deg Degree of term number= Integers which multiply the mean longitudes of the seven planets Mercury-Uranus in the argument. number= Integer multiplying precession accumulated from J2000 in the argument. --- CDS 1996 Jan 25 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 30-Oct-1995 J_AJ_110_1420.xml Hubble Space Telescope Planetary Camera observations of the stellar populations near the nucleus of M33 J/AJ/110/1649 J/AJ/110/1649 VI photometry near the M33 nucleus Hubble Space Telescope Planetary Camera observations of the stellar populations near the nucleus of M33 K J Mighell R M Rich Astron. J. 110 1649 1995 1995AJ....110.1649M Photometry Populations, stellar We have studied the stellar populations near the nucleus of the nearby spiral galaxy M33 using archival observations of the Hubble Space Telescope Planetary Camera in the F555W and F785LP passbands. The I vs (V-I) color-magnitude diagram reveals a young stellar population with a blue main sequence and red supergiants, and stars in a blue loop that are Cepheid candidates. An old red giant branch is clearly visible, with a break at I=20.7mag which is, within the observational errors, identical to the giant branch termination point of the Mould & Kristian (1986ApJ...305..591M) halo field. However, red giants are seen up to I=19.5mag, and many bright red giants are undetected in the V band. We find evidence for a wide abundance spread of at least 1.5dex from metal-poor (~M15) to metal-rich (>=47Tucanae) in the Population II stars, in sharp contrast to the M33 halo field of Mould & Kristian (1986ApJ...305..591M) which is metal-poor (~M92) with a narrow abundance range. We show that the various stellar populations have different spatial distributions. The Population II stars are more centrally concentrated than the Population I stars. The red giants brighter than I=20.7 (the termination point for a Galactic globular cluster giant branch) are found to be more centrally concentrated than the (presumably) old red giants. The most-centrally concentrated bright Population II giants are probably associated with the many bright red giants that are undetected in the V band. These infrared-bright giants were probably created in an intermediate-age burst of star formation that took place well after the formation of the oldest halo stars but long before the recent burst of star formation seen in nearby OB associations. This stellar population probably corresponds to the bulge identified in the infrared H band by Minniti et al. (1993ApJ...410L..79M).
HST
Photometry of stars near the nucleus of M33 ID Coded identification number=1 The left-most digit of the ID gives the PC chip number where the star may be found (5, 6, 7, or 8). The right-most 4 digits of the ID gives the x coordinate of the star multiplied by 10. The remaining 4 digits gives the y coordinate of the star multiplied by 10. All positions are given with respect to the W0M00104T data set. For example, the first star in Table 1 has an ID of 505142912 which indicates that it has the (x,y) position of (291.2, 51.4) on the PC5 CCD of the W0M00104T data set. --- F785LP F785LP (i) magnitude mag e_F785LP F785LP photometric error mag F555W F555W (v) magnitude mag e_F555W F555W photometric error mag Imag I magnitude mag V-I V-I color mag dRA Right ascension (J2000) offset number=2 Offsets in arcseconds from the nucleus of M33 (ID = 634043615) for the standard HST epoch of J2000.0. arcsec dDE Declination (J2000) offset number=2 Offsets in arcseconds from the nucleus of M33 (ID = 634043615) for the standard HST epoch of J2000.0. arcsec Class Photometric measurement class number=3 1 = v and i photometry (2532 stars) 2 = only i photometry (1028 stars) 3 = only v photometry (517 stars) --- table1.fit FITS BINTABLE version of table 1 CDS 1996 Jan 25 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 31-Oct-1995 J_AJ_110_1649.xml A 20cm VLA survey of Abell clusters of galaxies. V. Optical observations and surface photometry J/AJ/110/1959 J/AJ/110/1959 VLA survey of Abell clusters. V. A 20cm VLA survey of Abell clusters of galaxies. V. Optical observations and surface photometry M J Ledlow F N Owen Astron. J. 110 1959 1995 1995AJ....110.1959L Clusters, galaxy Photometry, surface We present results from a program of optical imaging of 265 radio galaxies in rich clusters. Using isophotal surface photometry, we investigate the optical properties such as the morphology, surface-brightness profiles, surface-brightness/size relationships, ellipticities, and the frequency of nonelliptical isophotes. The results are compared to a "normal" nonradio-selected sample of elliptical galaxies from the same clusters. The goal is to determine if the parent population of FR I radio galaxies can be distinguished optically from radio-quiet galaxies. The results of the analysis are that cluster ellipticals are a very homogeneous class of objects. The optical properties are consistent with a one-parameter family, where the optical luminosity is the fundamental parameter. In all tests considered, radio-loud FR I galaxies cannot be distinguished optically from radio-quiet galaxies selected from the same environment. The local density of nearby companions (<20kpc) and the frequency of morphological peculiarities or tidal interactions are not statistically different between the radio-loud and quiet samples. There is some suggestion from comparison to published samples of non-cluster radio galaxies, that the cluster environment is not condusive to long-lived tidal interactions, and that such events may be more important to galaxy evolution in poor groups and lower density environments. Such events appear to have little influence on the formation of FR I radio galaxies in rich clusters. The results are consistent with the idea that all elliptical galaxies may at some time (or many times) contain powerful (FR I) radio sources.
Results of surface photometry for z<0.09 sample Results of surface photometry for 0.09<z<0.20 sample Abell Abell number --- IAU IAU name in B1950 coordinates --- VmagGO m(GO) the apparent Gunn-Oke magnitude number=1 m(GO) the apparent Gunn-Oke magnitude (13.1kpc radius for H=75) mag VmagS m(S) the apparent Sandage magnitude number=2 m(S) the apparent Sandage magnitude (29.1kpc radius for H=75) mag mag24.5 m(24.5) the apparent isophotal magnitude number=3 m(24.5) the apparent isophotal magnitude measured to 24.5mag/arcsec^2^ in the rest-frame of the galaxy mag n_mag24.5 ma_24.5 is an estimated value number=4 An E appears if the isophotal magnitude value was estimated from figure 1 in this paper from the relationship between M(GO) and M(24.5). In this case, no surface-brightness profile was fit to the image. This occurred when a nearby galaxy or multiple nucleus was too difficult to remove. --- VMAGGO M(GO) absolute Gunn-Oke aperture mag. mag VMAGS M(S) absolute Sandage aperture mag. mag MAG24.5 M_24.5 absolute isophotal magnitude mag n_MAG24.5 M_24.5 is an estimated value number=4 An E appears if the isophotal magnitude value was estimated from figure 1 in this paper from the relationship between M(GO) and M(24.5). In this case, no surface-brightness profile was fit to the image. This occurred when a nearby galaxy or multiple nucleus was too difficult to remove. --- r24.5 Radius, 24.5 mag/arcsec2 isophote number=5 r(24.5) the radius in kpc measured at the 24.5mag/arcsec^2^ isophote (note that r=sqrt(ab) was used from the elliptical isophotal fits) kpc re de Vaucouleurs effective radius kpc eps Ellipticity, 24.5 mag/arcsec2 isophote --- PA Pos. angle, 24.5 mag/arcsec2 isophote deg sig_pl Std dev from power-law fit to profile number=6 sigma(pl) the standard deviation from a power-law least-squares fit to the surface-brightness profile --- sig_r Std dev from r^(1/4)^-law fit to profile number=7 sigma(r^1/4^) the standard deviation from a r^(1/4)^-law least-squares fit to the surface-brightness profile --- plexp Best-fitting power-law exponent number=8 The best-fitting power-law exponent to the surface-brightness profile --- l_N Limiting character for N --- N Number of points used in profile fitting number=9 The number of points used in the surface-brightness profile fitting --- table2.tex AASTeX version of table2.dat table3.tex AASTeX version of table3.dat CDS 1996 Jan 26 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 02-Nov-1995 UNKNOWN UNKNOWN * table2.dat : the extra '6' following mag24.5 value for row #139 was changed to a blank; * table3.dat : the extra 'f' preceding VmagGO in row #62, byte#15 was changed to a blank; J_AJ_110_1959.xml The IRAS Bright Galaxy Survey - Part II: Extension to Southern Declinations (Dec<=-30deg), and Low Galactic Latitudes (5<|b|<=30deg) J/AJ/110/1993 J/AJ/110/1993 IRAS Bright Galaxy Survey. II The IRAS Bright Galaxy Survey - Part II: Extension to Southern Declinations (Dec<=-30deg), and Low Galactic Latitudes (5<|b|<=30deg) D B Sanders E Egami S Lipari I F Mirabel B T Soifer Astron. J. 110 1993 1995 1995AJ....110.1993S VII/113 : Galaxies and QSOs observed in IRAS Survey (IPAC 1989) Galaxies, IR Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities >5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec<~-30deg, and low Galactic latitudes, 5deg<|b|<=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z<~0.1) Universe.
IRAS
Integrated flux densities of IRAS Bright Galaxies Integrated flux densities of IRAS bright Galaxies (5deg<|b|<10deg) Name Name The common catalog name has been taken in decreasing priority order from the NGC, UGC, ESO, IC, A, MCG, Zwicky catalog, Zwicky lists, Markarian, Arp-Madore, and IRAS catalogs. In table1b.dat, source IR 19542+1110 (RA=19:54:13.3, DE=+11:10:59) has a tentative identification of Halpha+[NII]; source not listed in NED. --- RAh Right Ascension (1950) All positions (1950) are taken from the PSC Version 2 <II/125> except for those galaxies from Rice et al <VII/109> where the positions were taken from the RC2. h RAm Right Ascension (1950) min RAs Right Ascension (1950) s DE- Sign Declination (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec cz Heliocentric radial velocity The heliocentric radial velocity (z=Delta(lambda(opt))/Lambda(opt) km/s u_cz Uncertainty flag for cz For those galaxies with no published redshift at the time the current survey was begun (1991), a velocity was measured from optical spectra obtained with either the UH 2.2 m telescope, or the 2.15 m telescope in Argentina. The typical uncertainty in the measured redshifts is +/- 30 km/s. All other redshifts are taken from NED. --- D Distance Either a "primary distance" from Sandage & Tammann <VII/51> catalog or a Fisher-Tully distance taken from either Aaronson et al. <VII/75>, Aaronson & Mould (1983ApJ...265....1A), or Tully & Shaya (1984ApJ...281...31T) (adjusted to a Virgo distance of 17.6 Mpc). For all other sources (those with no entry in D), the distance was calculated from CZ using the "Virgo-centric flow" model of Aaronson et al. (1982ApJ...258...64A) with an adopted distance to Virgo of 17.6 Mpc (corresponding to H0=75km/s/Mpc at large distances). Mpc m "Optical" magnitude The "optical" magnitude, as listed in the "object data" window in NED. For those few sources with more than one identified object within <~ 40" radius of the IRAS position (e.g. multiple "nuclei," close merger pairs), only the magnitude of the brightest object has been given. mag l_S12 S12 limiting character --- S12 Total 12 um IRAS flux density Best estimate for the total IRAS flux density as determined from coadded data using ADDSCAN/SCANPI. For the six sources not detected at 12 um, the reported upper limit is taken to be three times the rms noise of the coadded data. For source ESO 452-G005 (RA=16:28:33.5, DE=-27:59:48), it was impossible to estimate the 100 um flux. Jy n_S12 S12 note flag An asterisk (*) indicates that the flux density was taken directly from Rice et al. <VII/109>, while a hash mark (#) indicates that the source was partially blended with a nearby source, or that the baseline was somewhat uncertain and the listed flux has a correspondingly larger associated uncertainty, typically +/-10%-20% for sources at |b|>10deg, and +/-10%-30% for sources at |b|=5-10deg. --- e_S12 S12 rms noise of the coadded data mJy sS12 Size (extent) code for S12 The extent code: U = unresolved source, in which case the flux is taken as the point-source template fit; U+ = marginally resolved, and R = resolved, in which case the flux density is the integrated flux for the source. --- S25 Total 25 um IRAS flux density Jy n_S25 S25 note flag --- e_S25 S25 rms noise of the coadded data mJy sS25 Size (extent) code for S25 --- S60 Total 60 um IRAS flux density Jy n_S60 S60 note flag --- e_S60 S60 rms noise of the coadded data mJy sS60 Size (extent) code for S60 --- S100 Total 100 um IRAS flux density Jy n_S100 S100 note flag --- e_S100 S100 rms noise of the coadded data mJy sS100 Size (extent) code for S100 --- Data for extended sources Data for extended sources (5deg<|b|<10deg) Name Name as given in table 1 In table2b.dat, source IR 19542+1110 has a tentative identification and is not listed in NED. --- Band Wavelength for the following data um n_Band Band note flag An asterisk (*) indicates that the flux density was taken directly from Rice et al. <VII/109>, while a hash mark (#) indicates that the source was partially blended with a nearby source, or that the baseline was somewhat uncertain and the listed flux has a correspondingly larger associated uncertainty, typically +/-10%-20% for sources at |b|>10deg, and +/-10%-30% for sources at |b|=5-10deg. --- Res Resolution code, R or U+, as in table 1 --- Total The total flux density from table 1 Jy l_Templ Limiting character for Templ --- Templ Estimate from point-source template The estimate of the flux density from the amplitude of the point-source template. Jy u_Templ Templ uncertainty flag --- Peak Peak flux density The peak flux density in the average scan of the source (without the baseline fit used to determine the template fit). Jy W25 Source width at 25% peak flux density No attempt has been made to deconvolve the point-source width. arcmin W50 Source width at 50% peak flux density arcmin table1a.tex TeX version of table1a.dat table1b.tex TeX version of table1b.dat table2a.tex TeX version of table2a.dat table2b.tex TeX version of table2b.dat CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 19-Feb-1996 J_AJ_110_1993.xml Bright stars and recent star formation in the irregular Magellanic galaxy NGC 2366. J/AJ/110/212 J/AJ/110/212 BVR photometry of stars in NGC 2366 Bright stars and recent star formation in the irregular Magellanic galaxy NGC 2366. A Aparicio J Cepa C Gallart H O Castaneda C Chiosi G Bertelli J M Mas-Hesse C Munoz-Tunon E Telles G Tenorio-Tagle A I Diaz M L Garcia-Vargas F Garzon R M Gonzalez-Delgado E Perez J M Rodriguez-Espinosa E Terlevich R J Terlevich A M Varela J M Vilchez Astron. J. 110 212 1995 1995AJ....110..212A Photometry, CCD The stellar content of the Im galaxy NGC 2366 is discussed on the basis of CCD BVR photometry. The three brightest blue and red stars have been used to estimate its distance, obtaining a value of 2.9pc. The spatial distribution of the young stellar population is discussed in the light of the integrated color indices and the color-magnitude diagrams of different zones of the galaxy. A generalized star formation burst seems to have taken place about 50Myr ago. The youngest stars are preferentially formed in the South-West part of the bar, where the giant H II complex NGC 2363 is located, being younger and bluer. The bar seems to play a role favoring star formation in one of its extremes. Self-propagation however, does not seem to be triggering star formation at large scale. A small region, populated by very young stars has also been found at the East of the galaxy.
NGC 2366 07 28.7 +69 11 NGC 2363 07 28.4 +69 11
Photometry of stars in NGC 2363/66 Id Identification number --- Xpos CCD X position (from East to West) pix Ypos CCD Y position (from South to North) pix B-V B-V color index mag Vmag V magnitude mag V-R V-R color index mag Patricia Bauer CDS 1996 Apr 02 A. Aparicio, <aaj@ll.iac.es> J_AJ_110_212.xml The mass-to-light ratios of the Draco and Ursa Minor dwarf spheroidal galaxies. I. Radial velocities from multifiber spectroscopy. J/AJ/110/2131 J/AJ/110/2131 M/L for Draco and UMi. I. The mass-to-light ratios of the Draco and Ursa Minor dwarf spheroidal galaxies. I. Radial velocities from multifiber spectroscopy. T E Armandroff E W Olszewski C Pryor Astron. J. 110 2131 1995 1995AJ....110.2131A Clusters, galaxy Radial velocities We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.
Data for UMi stars Data for Draco stars Data for UMi non-member stars Data for Draco non-member stars Name Primary star name number=1 In tables 2 and 4: Numbers without prefix are Irwin UMi. Names starting by "N" are from Olsz, names with "q" are SOK COS### names are from the proper motion survey of Cudworth et al. (1986AJ.....92..766C) Names of the form ##q# are from the original iris photometry of Schommer, Olszewski, & Kunkel. Some of these have Van Agt (1967BAN....19..275V) numbers embedded in them. Although the ##q# designations are unpublished, they have been used in some previous studies. Most are cross-referenced in Cudworth et al. (1986AJ.....92..766C) and we give them only if there is no COS number. JI## names are from the work of H94. H94 also observed stars noted by Olszewski to be velocity members and stars from the COS list. Their designations seem to be mixed and matched; they called these stars CUD### and EDO###. We provide cross references to these names. Stars labelled N## are from an unpublished study by Olszewski. We suppress these names unless MMT velocities had been obtained using those names or unless the star was in our master list because of that unpublished study and because of the existence of MX spectra. Finally, almost every star has a 5-digit number. This number can be considered a running number; it is from a large body of APM photometry of the Ursa Minor region provided to us by M. Irwin. Although this photometry is unpublished, that is how we referred to the stars throughout the reduction. In table 3 and 5: Three-digit numbers and single letters are from Stetson (1979AJ.....84.1149S) photometry and proper motions. The star names are those of Baade and Swope (1961AJ.....66..300B), where a finding chart can be found. Four digit numbers are from the outer annulus of Stetson (private communication). He was able to derive good photometry, but could not derive proper motions. Roman numerals followed by a number are from the photographic photometry of McClure (private communication). Five digit numbers can be considered a running number; they are from a large body of APM photometry of the Draco region provided to us by M. Irwin. Although this photometry is unpublished, that is how we referred to the stars throughout the reduction. We remind readers that some mistakes may have crept into the cross-identifications; the coordinates are the ultimate way to settle any dispute. --- Num Number of velocities following header number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. --- RAh Right ascension, 1950 number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. h RAm Right ascension, 1950 number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. min RAs Right ascension, 1950 number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. s DE- Declination sign, always blank number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. --- DEd Declination, 1950 number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. deg DEm Declination, 1950 number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. arcmin DEs Declination, 1950 number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. arcsec <Vel> Average radial velocity number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. km/s e_<Vel> Uncertainty in <Vel> number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. km/s Chi2 Chi-square of scatter about <Vel> number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. --- Prob Probability of larger Chi2 number=2 The probability of obtaining a chi-square as large or larger than is observed if the star has a constant radial velocity. --- Other Other names for the star number= H94 claimed that the star COS390 (called CUD390 in H94) was a potential member of UMi based on a low-S/N spectrum. We report here a precise velocity showing that this star is not a member. --- Note Note number=3 1. C star 2. Identified as a giant candidate by MX spectroscopy 3. Observed by H94, but with low S/N. 4. H-beta in emission 5. Listed as EDOH and EDOE in Table 1 of H94 and as EDONH and EDONE in their Table 3 --- Velocities for UMi stars Velocities for Draco stars Velocities for UMi non-member stars Velocities for Draco non-member stars Name Primary star name --- JD Julian date of the velocity d Vel Measured radial velocity km/s e_Vel Uncertainty in Vel km/s R(Vel) R value for the velocity number=1 R is the ratio between the height of the peak of the correlation function and the rms noise in the correlation function. --- Src Source of the velocity number=2 The source of the velocity, where a blank indicates a velocity measured with Hydra and reported in this paper, an M indicates an MMT echelle velocity from Olszewski et al. (1995, AJ, 110, 2120), and an H indicates a velocity from Hargreaves et al. (1994, MNRAS, 271, 693). --- Lee Brotzman ADS James Marcout CDS 1996 Jan 26 UNKNOWN UNKNOWN The AAS CD-ROM original tables contained a mixture of data related to stars and velocity measurements; these were divided in two sets of files. In the course of this modification, a few errors were detected and corrected in the e_<Vel> column: table2s : N33 table5s: stars 14562 and 18411 e_<Vel> misaligned UNKNOWN UNKNOWN The stars in tables 2 and 4 are: <Irwin UMi NNNNN>, <Olsz ANN> (letter A = N), <SOK NNNqN>, The stars in tables 3 and 5 are: <Irwin Dra NNNNN>, <McClure R-NN> and <McClure CN> (Nos C1-C4), <Stetson NNNN> J_AJ_110_2131.xml Variable Stars in the Sextans Dwarf Spheroidal Galaxy J/AJ/110/2166 J/AJ/110/2166 Variables in Sextans dSph galaxy Variable Stars in the Sextans Dwarf Spheroidal Galaxy M Mateo P Fischer W Krzeminski Astron. J. 110 2166 1995 1995AJ....110.2166M Photometry, CCD Stars, variable We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.
Log of Sextans observations Frame Frame number --- Date UT Date of observation "DD/MM/YY" UTmidh Time of mid-exposure h UTmidm Time of mid-exposure min UTmids Time of mid-exposure s Exp Exposure time s AirMass Air-mass at mid-exposure --- HJD_mid HJD of mid exposure, epoch 2448000 --- Seeing Seeing arcsec Field Field, NE, NW, SE, SW --- Filt Filter, V or B --- B-band photometry of the Sextans variables Star Variable star number, V1, V2, ... V46 --- HJD Heliocentric Julian Date of observation --- Bmag B magnitude mag e_Bmag B magnitude error mag Phase Pulsation or orbital phase Pulsation or orbital phase calculated with the ephemerides in Table 4 of the printed paper. The phasing is defined so that phase zero corresponds to minimum light. No phase information is given for V16, V23, V35, or V46 because reliable periods could not be determined for these stars. --- V-band photometry of the Sextans variables Star Variable star number, V1, V2, ... V46 --- HJD Heliocentric Julian Date of observation --- Vmag V magnitude mag e_Vmag V magnitude error mag Phase Pulsation or orbital phase Pulsation or orbital phase calculated with the ephemerides in Table 4 of the printed paper. The phasing is defined so that phase zero corresponds to minimum light. No phase information is given for V16, V23, V35, or V46 because reliable periods could not be determined for these stars. --- Photometry of non-variable stars in the deep Sextans images Star Star number --- Xpos X coordinate pix Ypos Y coordinate pix Field Field, NE, NW, SE, SW --- RAh Right ascension 2000 h RAm Right ascension 2000 min RAs Right ascension 2000 s DE- Declination sign --- DEd Declination, 2000 (always "1") deg DEm Declination, 2000 arcmin DEs Declination, 2000 arcsec Vmag V magnitude mag e_Vmag V magnitude error mag B-V B-V color mag e_B-V B-V color error mag Patricia Bauer CDS 1996 Oct 24 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 03-Nov-1995 J_AJ_110_2166.xml The metallicities and kinematics of RR Lyrae variables. II. Galactic structure and formation from local stars J/AJ/110/2288 J/AJ/110/2288 Kinematics of local RR Lyrae stars. II. The metallicities and kinematics of RR Lyrae variables. II. Galactic structure and formation from local stars A C Layden Astron. J. 110 2288 1995 1995AJ....110.2288L J/AJ/108/1016 : Kinematics of local RR lyrae stars I. (Layden, 1994) Layden A.C., Paper III., 1995, AJ, 110, 2312 Proper motions Space, velocities Stars, variable We investigate the kinematics and spatial distribution of a sample of 302 nearby RR Lyrae variable stars with the goal of learning more about the formation history and present-day structure of the galaxy. We find that the kinematics change abruptly at [Fe/H]~-1.0. Above this value, the stars exhibit kinematic properties like those of other tracers of the galaxy's thick disk, while below [Fe/H]=-1.3, halo kinematics are observed. The stars with -1.3<=[Fe/H]<=-1.0 are a mixture of these populations, though the fraction of thick disk RR Lyrae stars with [Fe/H]<=-1.0 is significantly smaller than found among red giant stars by other authors; we discuss several possibilities for this discrepancy. The RR Lyraes with [Fe/H]>-0.5 exhibit somewhat cooler kinematics and a flatter spatial distribution than those of the thick disk, and may include some members of the old thin disk population. We find the kinematics of the halo RR Lyraes to be uncorrelated with abundance over the range -2.2<=[Fe/H]<=-1.0, and interpret this as evidence that the motions and chemical enrichment of gas in the early galaxy was characterized by a high degree of randomization, consistent with fragment accretion pictures of galaxy formation. We argue that the small number of thick disk stars with [Fe/H]<=-1.0 cannot be called upon to balance the net kinematics of a retrograde-rotating halo to produce the slow prograde rotations seen in this and other local samples; however, a hotter, slowly rotating, somewhat flattened second halo component may be consistent with kinematics both of local samples and of samples far from the galactic plane. We find the local density of halo RR Lyraes to be 11-15kpc^-3^, with a firm lower limit of 8+/-3kpc^-3^. This is larger than that predicted from counts of faint RR Lyraes far from the plane; either the flattening of the local halo is larger than c/a~0.7, or a two- component halo exists in which one component is quite flattened. We derive an exponential scale height of 0.7(+0.5)(-0.3)kpc and a midplane density of 10+/-4kpc^-3^ for the disk RR Lyraes with [Fe/H]>-1.0.
Proper motions and space velocities of 154 RR Lyrae variables Star Star name --- pmRA Proper motion in right ascension number=1 Proper motion in right ascension times the cosine of the declination, in arcsec/century 10-2arcsec/yr e_pmRA Error in pmRA 10-2arcsec/yr pmDE Proper motion in declination 10-2arcsec/yr e_pmDE Error in pmDE 10-2arcsec/yr Note Note flag number=2 a = proper motion from Hemenway (1975AJ.....80..199H) b = proper motion from Clube (1968, R. Obs. Bull. No. 136) c = proper motion from van Herk (1965BAN....18...71V) d = [Fe/H] taken from the literature --- Vrho Rho component of space velocity number=3 Space velocities were computed via the formulation of Johnson & Soderblom (1987AJ.....93..864J), which includes the treatment of errors. Many of the stars are sufficiently far from the Sun that the UVW coordinate system becomes misaligned with the principal galactocentric axes. Thus, the authors have rotated the UVW velocities of each star, and their errors, into the cylindrical frame, rho-phi-z. In this system, rho increases outward from the axis of galactic rotation, parallel to the galactic plane, phi is in the direction of galactic rotation, and z is toward the north galactic pole. km/s e_Vrho Error in Vrho km/s Vphi Phi component of space velocity number=3 Space velocities were computed via the formulation of Johnson & Soderblom (1987AJ.....93..864J), which includes the treatment of errors. Many of the stars are sufficiently far from the Sun that the UVW coordinate system becomes misaligned with the principal galactocentric axes. Thus, the authors have rotated the UVW velocities of each star, and their errors, into the cylindrical frame, rho-phi-z. In this system, rho increases outward from the axis of galactic rotation, parallel to the galactic plane, phi is in the direction of galactic rotation, and z is toward the north galactic pole. km/s e_Vphi Error in Vphi km/s Vz z component of space velocity number=3 Space velocities were computed via the formulation of Johnson & Soderblom (1987AJ.....93..864J), which includes the treatment of errors. Many of the stars are sufficiently far from the Sun that the UVW coordinate system becomes misaligned with the principal galactocentric axes. Thus, the authors have rotated the UVW velocities of each star, and their errors, into the cylindrical frame, rho-phi-z. In this system, rho increases outward from the axis of galactic rotation, parallel to the galactic plane, phi is in the direction of galactic rotation, and z is toward the north galactic pole. km/s e_Vz Error in Vz km/s [Fe/H] Metal abundance Sun CDS 1996 Jan 26 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 03-Nov-1995 J_AJ_110_2288.xml The composition of HB stars: RR Lyrae variables J/AJ/110/2319 J/AJ/110/2319 Abundances in RR Lyr variables The composition of HB stars: RR Lyrae variables G Clementini E Carretta R Gratton R Merighi J R Mould J K McCarthy Astron. J. 110 2319 1995 1995AJ....110.2319C Abundances Equivalent widths Stars, horizontal branch We have used moderately high-resolution, high S/N spectra to study the chemical composition of ten field ab-type RR Lyrae stars. Variables having accurate photometric and radial-velocity data were selected, in order to derive a precise estimate of the atmospheric parameters independently of excitation and ionization equilibria. A new temperature scale was determined from literature "Infrared Flux Method" measures of subdwarfs and the Kurucz (1992) (priv. com.) model atmospheres, and used to calibrate colors for both dwarfs and RR Lyraes. Photometric reddening estimates for the program stars were carefully examined, and compared with other determinations. The applicability of Kurucz (1992) (priv. com.) model atmospheres in the analysis of RR Lyraes at minimum light was analyzed: we found that they are able to reproduce colors, excitation, and ionization equilibria as well as the wings of Halpha. The comparison solar abundances were carefully determined. From a new analysis of weak Fe I lines with accurate gfs [Bard & Kock, A&A, 282, 1014 (1994)] we derived log epsilon(Fe)_Sun=7.52, in agreement with the Fe abundances determined from meteorites and Fe II lines. We derived abundances for 21 species. Main results are: The metal abundances of the program stars span the range -2.50<[Fe/H]<+0.17. Lines of most elements are found to form in LTE conditions. Fe lines satisfy very well the excitation and ionization equilibria. A comparison with statistical equilibrium computations shows that rather large collisional cross sections are required to reproduce observations. If these cross sections are then used in the analysis of the formation of Fe lines in subdwarfs and RGB stars, no significant departures from LTE are found for these stars, thus validating the very numerous LTE analyses. RR Lyraes share the typical abundance pattern of other stars of similar [Fe/H]: alpha-elements are overabundant by ~0.4dex and Mn is underabundant by ~0.6dex in stars with [Fe/H]<-1. Solar scaled abundances are found for most of the other species, except for the low Ba abundance in the extremely metal-poor star X Ari ([Fe/H]~-2.5). Significant departures from LTE are found for a few species: Nd II, Ce II, Y II, and Sc II are severely underabundant (~0.5dex) in metal-rich variables; Ti I and Cr I are slightly (~0.1-0.2dex) underabundant in metal-poor stars. These effects are attributed to overionization. We suggest that the photoionization of the alkaline earth-like ions is due to Lyman lines emission produced by the shock waves that propagate in the atmosphere of these variables [Fokin (1992MNRAS.256...26F)]. Departures from LTE were considered in detail in the derivation of abundances for the light elements (O and Na). Significant corrections were required for the O I IR triplet and the Na D lines. The resulting pattern reproduces that observed in less evolved field stars. We did not find any evidence for an O-Na anticorrelation among these field HB stars, suggesting that the environment is likely to be responsible for the anticorrelation found in metal-poor globular cluster stars [Sneden et al. =1992AJ....104.2121S]. We used our new [Fe/H] abundances, as well as values from Butler and co-workers (corrected to our system), and from high- resolution spectroscopy of globular clusters giants, to obtain a revised calibration of the low-resolution metallicity index Delta(S) [Preston =1959ApJ...130..507P]: [Fe/H]=-0.194(+/-0.011)Delta(S)-0.08(+/-0.18). Our new metallicity scale is stretched on both low and high metallicity ends with respect to Butler's [1975ApJ...200...68B]. The error in [Fe/H] by Delta(S) observations is 0.16dex, well of the same order of high-resolution metallicity determinations. The slope of the calibration obtained considering only stars with 4<Delta(S)<10 is slightly smaller than that obtained using all stars. While this difference is only barely significant, it might point out the presence of a nonlinearity of the Delta(S) vs [Fe/H] relation, as suggested by Manduca [ApJ, 245, 258 (1981)]. The new [Fe/H] values were used to update the metallicity calibration of the Ca II K line index [Clementini et al. =1991AJ....101.2168C]. Using the present new metallicities, and W'(K) values and relative errors from Clementini et al. (1991), a least-squares fit weighted both in W'(K) and [Fe/H] gives [Fe/H]=0.65(+/-0.17)W'(K)-3.49(+/-0.39). Finally, our new metallicity scale was used to revise the metallicity dependence of the absolute magnitude of RR Lyrae stars, M_V. Using M_V values from Fernley [1994A&A...284L..16F] for the field stars, and estimates from Liu & Janes [1990ApJ...360..561L] and Storm et al. [1994A&A...290..443S] for the cluster variables, we found M_V=0.20(+/-0.03) [Fe/H]+1.06(+/-0.04) and M_V=0.19(+/-0.03)[Fe/H]+0.96(+/-0.04), the last being obtained by using M_V estimates derived for a value of the conversion factor between observed and true pulsation velocity p=1.38 (Fernley 1994). The adoption of the new metallicity scale does not yield significant changes in the slope or zero point of the M_V vs [Fe/H] relation. Observations do not rule out the possibility that the slope of the M_V vs [Fe/H] relation might be different for metal-poor and metal-rich variables. However, a larger sample of Baade-Wesselink M_V determinations is required to definitely settle this question.
RR Cet HD 9356 01 32 08.1 +01 20 32 RR Lyr HD 182989 19 25 28.3 +42 47 14 ST Boo 15 30 39 +35 47 00 SW And 00 23 43.0 +29 24 04 UU Cet 00 04 04 -16 59 48 V440 Sgr 19 32 18.9 -23 51 30 V445 Oph 16 24 41 -06 32 06 VX Her 16 30 41 +18 21 42 VY Ser HD 138279 15 31 02.1 +01 41 02 X Ari HD 19510 03 08 30.6 +10 26 50
List of lines and adopted gf values and their equivalent widths Element Element --- Lambda Wavelength 0.1nm EP Energy potential eV loggf Oscillator strength --- EWRRCet Equivalent width for RR Cet 0.1nm lognRRCet Abundance for RR Cet Sun EWRRLyr Equivalent width for RR Lyr 0.1nm lognRRLyr Abundance for RR Lyr Sun EWSTBoo Equivalent width for ST Boo 0.1nm lognSTBoo Abundance for ST Boo Sun EWSWAnd Equivalent width for SW And 0.1nm lognSWAnd Abundance for SW And Sun EWUUCet Equivalent width for UU Cet 0.1nm lognUUCet Abundance for UU Cet Sun EWV440Sgr Equivalent width for V440 Sgr 0.1nm lognV440Sgr Abundance for V440 Sgr Sun EWV445Oph Equivalent width for V445 Oph 0.1nm lognV445Oph Abundance for V445 Oph Sun EWVXHer Equivalent width for VX Her 0.1nm lognVXHer Abundance for VX Her Sun EWVYSer Equivalent width for VY Ser 0.1nm lognVYSer Abundance for VY Ser Sun EWXAri Equivalent width for X Ari 0.1nm lognXAri Abundance for X Ari Sun CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 19-Feb-1996 J_AJ_110_2319.xml Observations and analysis of the field contact binary V728 Herculis J/AJ/110/2400 J/AJ/110/2400 BVI photometry of V728 Her Observations and analysis of the field contact binary V728 Herculis R H Nelson E F Milone J Van Leeuwen D Terrell J E Penfold J Kallrath Astron. J. 110 2400 1995 1995AJ....110.2400N Photometry Stars, variable The W UMa system V728 Her has been observed photometrically in B, V, and I_c passbands at the RAO over five seasons and spectroscopically at DAO over three seasons to obtain radial velocities. New times of minima are provided and a period analysis confirms previous ephemerides. The light and radial velocity curves were analyzed with the latest University of Calgary enhancements to the Wilson-Devinney program and new solutions found. The best model is that involving a contact system with convective atmospheres. In probing the best solution possible, use was made of the enhanced reflection and second-order limb-darkening calculations available in the 1993 version of the WD program. The mass ratio is found to be 0.1786+/-0.0023. The contact parameter is found to be f=0.71+/-0.11. The masses are determined to be 1.654+/-0.037M_{sun}_ and 0.295+/-0.009M_{sun}_ and the radii are 1.784+/-0.015R_{sun}_ and 0.867+/-0.054R_{sun}_, respectively. The determined temperature difference, T2-T1 is 165+/-19K, and the luminosities for components 1 and 2 are 5.5+/-0.5L_{sun}_ and 1.4+/-0.3L_{sun}_, respectively.
V728 Her 17 18 04.4 +41 50 40
V728 Her photoelectric observations HJD-2440000 Heliocentric Julian Day number - 2440000 d Phase Phase Phase computed according to E0 = 2446949.83672, P=0.4712866 d --- Bmag (Var-comp.) differential Johnson B mag mag Vmag (Var-comp.) differential Johnson V mag mag Icmag (Var-comp.) differential Cousins I mag mag CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 1-May-1996 J_AJ_110_2400.xml Red and infrared polarimetry of highly reddened stars in the galactic plane. J/AJ/110/268 J/AJ/110/268 Red and infrared polarimetry in galactic plane Red and infrared polarimetry of highly reddened stars in the galactic plane. M Creese T J Jones H A Kobulnicky Astron. J. 110 268 1995 1995AJ....110..268C Photometry, infrared Polarization We present VRIJHK polarimetry and JHK photometry of highly reddened stars found in an objective prism survey published by Stephenson (1992AJ....103..263S). The JHK colors of these stars are consistent with interstellar extinction as the dominant source of the reddening. The distribution of the polarization position angles in Galactic coordinates is very similar to previous optical polarimetry surveys such as Mathewson & Ford ([MNRAS, 74, 139 (1970)]. However, for the redder stars with IR polarimetry, the polarization strength is moderately lower than expected for the amount of extinction. We postulate that the line of sight to many of these stars samples specific regions where the grain population has poor polarizing properties, while the remainder of the line of sight is similar to the paths sampled by previous optical surveys. The wavelength dependence of the polarization from 1-2.5{mu}m for this sample of stars shows weak evidence for a greater departure from the mean for interstellar polarization than for most published near-infrared polarimetry.
VRIJHK polarimetry Star Star number from Stephenson (1992) --- PolV Polarisation in V filter % e_PolV rms uncertainty on PV % PAV Position angle in V filter deg PolR Polarisation in R filter % e_PolR rms uncertainty on PR % PAR Position angle in R filter deg PolI Polarisation in I filter % e_PolI rms uncertainty on PI % PAI Position angle in I filter deg PolJ Polarisation in J filter % e_PolJ rms uncertainty on PJ % PAJ Position angle in J filter deg PolH Polarisation in H filter % e_PolH rms uncertainty on PH % PAH Position angle in H filter deg PolK Polarisation in K filter % e_PolK rms uncertainty on PK % PAK Position angle in K filter deg R band polarimetry Star Star number from Stephenson (1992) --- PolR Polarimetry in R filter % e_PolR rms uncertainty on PR % PAR Position angle in R filter deg JHK photometry Star Star number from Stephenson (1992) --- Jmag J magnitude mag e_Jmag rms uncertainty on J magnitude mag Hmag H magnitude mag e_Hmag rms uncertainty on H magnitude mag Kmag K magnitude mag e_Kmag rms uncertainty on K magnitude mag Patricia Bauer CDS 1996 Apr 04 Terry Jones <tjj@astro.spa.umn.edu> J_AJ_110_268.xml Hot, luminous stars in selected regions of NGC 6822, M31 and M33 J/AJ/110/2715 J/AJ/110/2715 UBV photometry in NGC 6822, M31 and M33 Hot, luminous stars in selected regions of NGC 6822, M31 and M33 P Massey T E Armandroff R Pyke K Patel C D Wilson Astron. J. 110 2715 1995 1995AJ....110.2715M Photometry, UBV Stars, luminous We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (>80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass >40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (>40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.
Photometry of NGC 6822 stars Photometry of M33 stars Star Star identification --- RAh Right Ascension (2000) h RAm Right Ascension (2000) min RAs Right Ascension (2000) s DE- Declination sign (2000) --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Vmag V magnitude mag U-B U-B color mag B-V B-V color mag Q Q = U-B - 0.72x(B-V) mag Comment Spectral type, cross id's and/or comments References for cross-id's: NGC6822 CW: Wilson (1992AJ....104.1374W) WR=Wolf-Rayet from Armandroff & Massey (1985ApJ...291..685A) M33 B or HS are id's from Humphreys & Sandage (1980ApJS...44..319H) RW=Regan & Wilson (1993AJ....105..499R) --- CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 19-Feb-1996 J_AJ_110_2715.xml The absolute proper motion and a membership survey of the Sculptor dwarf spheroidal galaxy J/AJ/110/2747 J/AJ/110/2747 Stars in Sculptor dwarf spheroidal galaxy The absolute proper motion and a membership survey of the Sculptor dwarf spheroidal galaxy A E Schweitzer K M Cudworth S R Majewski N B Suntzeff Astron. J. 110 2747 1995 1995AJ....110.2747S Cross identifications Proper motions Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.
Sculptor photometry, membership probabilities, positions, and proper motions Photometry and positions of possible variable stars in Sculptor SCMS Identification from this study --- V78 ID from Van Agt, 1978PDDO....3..205V --- H65 ID from Hodge, 1965ApJ...142.1390H --- KD77 ID from Kunkel & Demers, 1977ApJ...214...21K --- FBM82 ID from Frogel et al., 1982ApJ...252..133F --- Vmag V magnitude mag B-V B-V color index mag PMemb Probability of membership Probability of membership, only for table3.dat. The background galaxies, for which the stellar profile-fitting photometry may be unreliable, are listed at the beginning with a membership probability of -1. % Xpos X coordinate relative to dSph center arcsec Ypos Y coordinate relative to dSph center arcsec RAh Right Ascension (2000) h RAm Right Ascension (2000) min RAs Right Ascension (2000) s DE- Declination sign (2000) --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec pmX Relative proper motion 10-2mas/yr e_pmX Standard error in pmX 10-2mas/yr pmY Relative proper motion 10-2mas/yr e_pmY Standard error in pmY 10-2mas/yr CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 14-Jul-1996 J_AJ_110_2747.xml Infrared array photometry of metal-rich globular clusters. III. Two more clusters and an analysis of V-K colors. J/AJ/110/2844 J/AJ/110/2844 JHK photometry of globular clusters. III. Infrared array photometry of metal-rich globular clusters. III. Two more clusters and an analysis of V-K colors. L E Kuchinski J A Frogel Astron. J. 110 2844 1995 1995AJ....110.2844K J/AJ/109/1131 : Paper I: clusters NGC 5927, Terzan 2, NGC 6712, NGC 6838 J/AJ/109/1154 : Paper II: cluster Liller 1. Schechter et al. 1993 PASP 105, 134 Clusters, globular Photometry, infrared We present new JHK photometry for the disk globular clusters NGC 6440 and NGC 6624. These data are initially used to confirm and refine several important results from Kuchinski et al. (1995AJ....109.1131K) for other disk globular. First, we again demonstrate the ability to derive a reddening-independent estimate for the [Fe/H] of a cluster from the slope if its giant branch (GB) in a K, J-K color magnitude diagram (CMD). Second, the reddening corrected J-K color and K magnitude of the center of the horizontal branch (HB) and the J-K color of its red edge are confirmed to be independent of [Fe/H] for these clusters. Thus these parameters can be used to estimate E(J-K) of metal-rich clusters with no knowledge of distance or [Fe/H] and to estimate (m-M) if one can first estimate the reddening. We also confirm that the reddening-independent quantities, the half width of a cluster's horizontal branch (HB), and the color difference between the center of the HB and the GB at the level of the HB, both appear to be insensitive to metallicity. The JHK colors of NGC 6440 are similar to those of Liller 1; in both cases these colors are unlike those seen for other globular clusters, field giants, or bulge giants. We have not been able to identify any other cluster parameter that would help to explain these anomalous colors. We have assembled V photometry from the literature for the clusters in our sample and VK photometry for two additional disk globular clusters from Davidge et al. (1992ApJS...81..251D). We conclude that K, J-K CMDs are preferable to K, V-K CMDs as tools to study basic cluster properties. Finally, we compare our data with theoretical isochrones for metal-rich clusters and present observational evidence that the dependence of the V-K color of the GB on [Fe/H] may be different for halo and disk globular clusters. This difference may be related to differences in the [O/Fe] values for the two cluster systems.
NGC 5927 15 27.6 -50 39 NGC 6624 18 23.6 -30 21 NGC 6440 17 48.9 -20 22 NGC 6712 18 53.0 -08 43 M 71 NGC 6838 19 53.7 +18 47
NGC 6624 data NGC 6440 data ID Identification number --- Xpos X coordinate (from East to West) number=1 the plate scale is 0.35"/pix. pix Ypos Y coordinate (from South to North) number=1 the plate scale is 0.35"/pix. pix Kmag K magnitude mag J-K J-K color index mag H-K H-K color index mag V-K V-K color index mag Code Exposure code number=2 3 = 3s exposure, 10 = 10s exposure, 20 = 20s exposure 203 = color data from both sets (3s and 20s) (table3 only) --- Note Notes number=3 NO = star with DoPhot error >=0.06mag (DoPhot, Schechter et al. 1993) --- NGC 5927 data NGC 6712 data M 71 data ID Identification number --- Kmag K Magnitude mag V-K V-K color index mag Patricia Bauer CDS 1996 Aug 09 Leslie E. Kuchinski <lek@payne.mps.ohio-state.edu> J_AJ_110_2844.xml The Shapley supercluster. I. Spectroscopic observations in the central region J/AJ/110/463 J/AJ/110/463 Kinematics of the Shapley supercluster The Shapley supercluster. I. Spectroscopic observations in the central region H Quintana A Ramirez J Melnick S Raychaudhury E Slezak Astron. J. 110 463 1995 1995AJ....110..463Q Clusters, galaxy Radial velocities We present a new analysis of the kinematics of the Shapley supercluster based on radial velocities for 1087 galaxies in the clusters A3558 (Shapley 8), A3528 (Klemola 21), A3532 (Klemola 22), A3530, A3556 (SC 1321-314), A3559 (CE 1327-292), A3560, A3562, SC 1329-314 and in the intercluster region of the core of the supercluster, of which 367 are new measurements. We also present accurate positions from APM and MAMA scans of the ESO/SERC Southern Sky Survey photographic plates. We obtain new velocity dispersions and estimate the masses of the member clusters, evaluating dynamical models of the supercluster. The supercluster is found to be significantly flattened. We find that for Omega_0=0.3, H_0=75km/s/Mpc, the gravitational pull of the supercluster may account for up to 25% of the peculiar velocity of the Local Group required to explain the dipole anisotropy of the Cosmic Microwave Background radiation, in which case the mass of the supercluster would be dominated by intercluster dark matter. This fractional contribution would be considerably higher for combinations of significantly lower values of Omega_0 and higher values of H_0.
Galaxy velocities Region ACO <VII/110> cluster name or cluster area code number=1 Gives either the ACO <VII/110> cluster name, ordered by ascending number, or a code for the area where the cluster is located. These areas denote (1degree x 5min) regions (approx 1 square degree) in which we divided the field to program the observations, and are named by the coordinates of the NW corner. --- ID Observing identifications --- ESO ESO field --- Coord APM, MAMA cat. numbers or other codes number=2 The APM, MAMA catalogue numbers or other codes used as source for coordinates. Most coordinates are either from digital scans of the SERC IIIa-J atlas, using the APM facility in Cambridge, England or from scans of ESO/SRC R fields done with the MAMA machine at Paris. For galaxies not found in the APM and MAMA scans, positions are quoted from the ESO/Uppsala catalog (Lauberts 1982, <VII/34>). Coordinates for galaxies in A3558 were measured with the Optronics machine at ESO, Garching. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec u_RAh Equatorial coordinate uncertainty flag --- Code Codes for following fields number=3 R = m_J is R magnitude from the MAMA survey. : = m_J is uncertain (saturated image on plate or estimated by eye) < = m_J is an upper limit (the magnitude quoted being the total magnitude of a merged image of which the galaxy is a part) ( = velocities are not used in the mean values of redshifts. --- Jmag Ptg. J mag, measured from APM survey mag RV Heliocentric velocities km/s e_RV Heliocentric velocities error km/s R R value or number of lines number=4 The R value of the cross-correlation, or the number of lines measured in each spectra, if the line position method was used. The R value is a real value and the number of lines is an integer value. --- Ref Code for observer or velocity reference number=5 The code of observer/telescope/date or a reference code if the galaxy also has a velocity reported in the literature. Q1-Q7,M1-M3: observing sessions as in Table 1 of the printed paper. MGS87 Metcalfe et al. (1987MNRAS.225..581M) TCG90 Teague et al. (1990ApJS...72..715T) Da86 da Costa et al. (1986AJ.....91....6D) Da87 da Costa et al. (1987AJ.....93.1338D) DS88 Dressler and Shectman 1988, AJ, 95, 284 D091 Dressler 1991 <J/ApJS/75/241> Cr87 Cristiani et al. (1987A&A...179..108C) R087 Richter, O.-G. (1987A&AS...67..261R) Ve90 Vettolani et al. (1990AJ.....99.1709V) Mo88 Monk et al. (1988MNRAS.234..193M) Mo89 Mould et al. (1989ApJ...338..654A) PGC Paturel et al. Catalogue of Principal Galaxies, Monographies de la Base de Donnees Extragalactiques, No 1, Lyon: Obs. de Lyon; 1737 ZCAT Catalog, Huchra et al. 1993 <VII/164> --- CDS 1996 Jan 10 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 06-Oct-1995 J_AJ_110_463.xml The LMC cluster NGC 1866. I. A revised photometric sequence and a reconnaissance of the surrounding field population J/AJ/110/638 J/AJ/110/638 BVI photometry in NGC 1866 The LMC cluster NGC 1866. I. A revised photometric sequence and a reconnaissance of the surrounding field population A R Walker Astron. J. 110 638 1995 1995AJ....110..638W Clusters, globular Photometry A photometric sequence consisting of 53 stars measured in the V, B, and I bands has been set up in the vicinity of the rich, young Large Magellanic Cloud cluster, NGC 1866. Many of these stars are relatively isolated and are thus suitable for use as local standard stars for photometric studies of the cluster. Color magnitude diagrams to a limit of V=20.5 for various parts of the 13x13arcmin field, centered on the cluster, show that NGC 1866 is embedded in a mix of populations which includes stars younger than the cluster itself, the dominant 0.5-3Gyr population, plus some very old stars represented by four RR Lyrae variables.
Photometry for 6442 stars in a field centered on NGC 1866 Star Star number --- Xpos X coordinate pix Ypos Y coordinate pix Vmag V magnitude mag B-V B-V color mag V-I V-I color mag e_Vmag Error in Vmag mag e_B-V Error in B-V mag e_V-I Error in V-I mag o_Vmag Number of V observations --- o_B-V Number of B observations --- o_V-I Number of I observations --- CDS 1996 Jan 10 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 27-Sep-1995 J_AJ_110_638.xml A VIc color-magnitude diagram of the globular cluster NGC 6352 from Hubble Space Telescope Planetary Camera observations J/AJ/110/652 J/AJ/110/652 VI photometry in NGC 6352 A VIc color-magnitude diagram of the globular cluster NGC 6352 from Hubble Space Telescope Planetary Camera observations L K Fullton B W Carney E W Olszewski R Zinn P Demarque K A Janes G S Da Costa P Seitzer Astron. J. 110 652 1995 1995AJ....110..652F Clusters, globular Photometry Tables CD-1, CD-2, and CD-3 contain the photometric data used to generate the color-magnitude diagrams in the printed paper. The tables themselves were not printed in the paper, but were provided by the authors for publication on the AAS CD-ROM Series. The globular cluster NGC 6352, which on the basis of its Galactic position, radial velocity, and [Fe/H] is a member of the (thick) disk system of globular clusters, has been observed to below the main-sequence turnoff (MSTO) using the Hubble Space Telescope. These observations, which were obtained before the repair mission, were analyzed using the flux-conserving iterative/recursive deconvolution algorithm developed at the University of North Carolina. This algorithm can produce more precise photometry than standard PSF-fitting methods with the aberrated images. The V, (V-Ic) color-magnitude diagram constructed from these observations places the cluster turnoff at V=18.80+/-0.10. Observations with the CTIO 0.9m telescope have been used to photometer the brighter stars in the cluster, providing a calibration of the HST data and an estimate of the cluster's reddening, E(B-V)=0.21+/-0.03. From spectroscopic observations of the strengths of the Ca II triplet lines in red giants in the cluster and from previous measurements in the literature, we find that NGC 6352 is only slightly more metal rich (Delta[Fe/H]=0.08+/-0.05) than the prototypical disk globular cluster, 47 Tuc. From the difference in V magnitude between the horizontal branch and the MSTO, we find that NGC 6352 is essentially the same age as 47 Tuc (formally, older by 0.7+/-2.2Gyr). Comparisons with the latest Yale isochrones support this result and yield 14.5+/-2Gyr for the age of 47 Tuc from the photometry of Hesser et al. (1987PASP...99..739H), which is consistent with other determinations. The old age obtained for NGC 6352 provides additional evidence that the disk system of globular clusters is very old and is in fact older or comparable in age to several globular clusters populating the Galactic halo.
HST
Ground-based data ID Star identification --- SN Cross-id from Sarajedini & Norris (1994ApJS...93..161S) --- Xpos X coordinate pix Ypos Y coordinate pix Vmag V magnitude mag e_Vmag Sigma of Vmag measurement mag V-Ic V-Ic color mag e_V-Ic Sigma of V-Ic measurement mag HST cluster data HST comparison field data Chip Chip number --- ID Star identification number --- n_ID Indicates no other star on the frame within 15 pixels --- Xpos X coordinate pix Ypos Y coordinate pix Vmag V magnitude mag e_Vmag Sigma of Vmag measurement mag V-Ic V-Ic color mag e_V-Ic Sigma of V-Ic measurement mag CDS 1996 Jan 10 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 27-Sep-1995 J_AJ_110_652.xml The RR Lyrae Variable Stars in the Globular Cluster M15 J/AJ/110/704 J/AJ/110/704 RR Lyrae Variables in M15 The RR Lyrae Variable Stars in the Globular Cluster M15 N A Silbermann A Smith Horace Astron. J. 110 704 1995 1995AJ....110..704S J/AJ/106/154 : HST Observations in inner region of M15 (Ferraro+ 1993) J/AJ/107/1745 : HST UVI photometry of M15. II. (Yanny+, 1994) J/AJ/107/2067 : Fabry-Perot measurements of M15 (Gebhardt+, 1994) J/ApJ/347/251 : Dynamics of Globular Cluster M15 (Peterson+ 1989) Sandage A., Katem B., Sandage M., =1981ApJS...46...41S Bingham E.A., Cacciari C., Dickens R.J., Fusi Pecci F., =1984MNRAS.209..765B Clusters, globular Photometry, CCD Stars, variable New CCD photometry is presented for RR Lyrae variable stars in the globular cluster M15. This photometry, mainly in V and R, with some additional B and I, is used to construct lightcurves of 44 RR Lyraes and one Cepheid in M15. One new low-amplitude RR Lyrae star was discovered. The observable parameters of the light curves are used, in conjunction with theoretical photometric indices, to obtain effective temperatures and bolometric magnitudes in the RR Lyrae stars. We confirm that the regions occupied by RRab and RRcd variables in M15 have little or no overlap in effective temperature. Photometry for variable and nonvariable horizontal branch stars in M15 is used to establish the high and low temperature boundaries of the instability strip. There is evidence that the blue edge of the M15 RR Lyrae instability strip becomes cooler at higher luminosities. Employing Cox's value of the mass of RRd stars, 0.75 Msun, and the pulsation equation, the absolute magnitude of the RR Lyrae stars in M15 is estimated to be <M_V_> = +0.36+/-0.12 mag. However, this result depends upon the adopted mass, bolometric correction, and color-temperature relation, which remain significantly uncertain. The implications of the absolute magnitude determination for the ages of the globular clusters are discussed.
M 15 NGC 7078 C 2127+119 21 29 58.2 +12 10 02
MSU V photometry of M15 variables MSU R photometry of M15 variables Frame Frame --- HJD-2448000 Heliocentric Date of Observation - 2448000 d V1 MSU photometry for star V1 mag u_V1 Uncertainty flag on V1 --- V2 MSU photometry for star V2 mag u_V2 Uncertainty flag on V2 --- V3 MSU photometry for star V3 mag u_V3 Uncertainty flag on V3 --- V4 MSU photometry for star V4 mag u_V4 Uncertainty flag on V4 --- V5 MSU photometry for star V5 mag u_V5 Uncertainty flag on V5 --- V6 MSU photometry for star V6 mag u_V6 Uncertainty flag on V6 --- V7 MSU photometry for star V7 mag u_V7 Uncertainty flag on V7 --- V8 MSU photometry for star V8 mag u_V8 Uncertainty flag on V8 --- V9 MSU photometry for star V9 mag u_V9 Uncertainty flag on V9 --- V10 MSU photometry for star V10 mag u_V10 Uncertainty flag on V10 --- V11 MSU photometry for star V11 mag u_V11 Uncertainty flag on V11 --- V13 MSU photometry for star V13 mag u_V13 Uncertainty flag on V13 --- V14 MSU photometry for star V14 mag u_V14 Uncertainty flag on V14 --- V15 MSU photometry for star V15 mag u_V15 Uncertainty flag on V15 --- V17 MSU photometry for star V17 mag u_V17 Uncertainty flag on V17 --- V18 MSU photometry for star V18 mag u_V18 Uncertainty flag on V18 --- V19 MSU photometry for star V19 mag u_V19 Uncertainty flag on V19 --- V20 MSU photometry for star V20 mag u_V20 Uncertainty flag on V20 --- V22 MSU photometry for star V22 mag u_V22 Uncertainty flag on V22 --- V23 MSU photometry for star V23 mag u_V23 Uncertainty flag on V23 --- V24 MSU photometry for star V24 mag u_V24 Uncertainty flag on V24 --- V25 MSU photometry for star V25 mag u_V25 Uncertainty flag on V25 --- V29 MSU photometry for star V29 mag u_V29 Uncertainty flag on V29 --- V30 MSU photometry for star V30 mag u_V30 Uncertainty flag on V30 --- V31 MSU photometry for star V31 mag u_V31 Uncertainty flag on V31 --- V32 MSU photometry for star V32 mag u_V32 Uncertainty flag on V32 --- V35 MSU photometry for star V35 mag u_V35 Uncertainty flag on V35 --- V38 MSU photometry for star V38 mag u_V38 Uncertainty flag on V38 --- V39 MSU photometry for star V39 mag u_V39 Uncertainty flag on V39 --- V40 MSU photometry for star V40 mag u_V40 Uncertainty flag on V40 --- V42 MSU photometry for star V42 mag u_V42 Uncertainty flag on V42 --- V44 MSU photometry for star V44 mag u_V44 Uncertainty flag on V44 --- V49 MSU photometry for star V49 mag u_V49 Uncertainty flag on V49 --- V50 MSU photometry for star V50 mag u_V50 Uncertainty flag on V50 --- V51 MSU photometry for star V51 mag u_V51 Uncertainty flag on V51 --- V52 MSU photometry for star V52 mag u_V52 Uncertainty flag on V52 --- V53 MSU photometry for star V53 mag u_V53 Uncertainty flag on V53 --- V54 MSU photometry for star V54 mag u_V54 Uncertainty flag on V54 --- V65 MSU photometry for star V65 mag u_V65 Uncertainty flag on V65 --- V66 MSU photometry for star V66 mag u_V66 Uncertainty flag on V66 --- V67 MSU photometry for star V67 mag u_V67 Uncertainty flag on V67 --- V74 MSU photometry for star V74 mag u_V74 Uncertainty flag on V74 --- V97 MSU photometry for star V97 mag u_V97 Uncertainty flag on V97 --- V99 MSU photometry for star V99 mag u_V99 Uncertainty flag on V99 --- V113 MSU photometry for star V113 mag u_V113 Uncertainty flag on V113 --- WIRO south field B photometry of M15 variables WIRO south field V photometry of M15 variables WIRO south field R photometry of M15 variables WIRO south field I photometry of M15 variables Frame Frame number --- HJD-2448000 Heliocentric Date of Observation - 2448000 d V3 WIRO south field phot. for star V3 mag V4 WIRO south field phot. for star V4 mag V5 WIRO south field phot. for star V5 mag V11 WIRO south field phot. for star V11 mag V12 WIRO south field phot. for star V12 mag V13 WIRO south field phot. for star V13 mag V14 WIRO south field phot. for star V14 mag V15 WIRO south field phot. for star V15 mag V35 WIRO south field phot. for star V35 mag V38 WIRO south field phot. for star V38 mag V39 WIRO south field phot. for star V39 mag V40 WIRO south field phot. for star V40 mag V42 WIRO south field phot. for star V42 mag V52 WIRO south field phot. for star V52 mag V53 WIRO south field phot. for star V53 mag V66 WIRO south field phot. for star V66 mag V74 WIRO south field phot. for star V74 mag V113 WIRO south field phot. for star V113 mag WIRO NW field B photometry of M15 variables WIRO NW field V photometry of M15 variables WIRO NW field R photometry of M15 variables WIRO NW field I photometry of M15 variables Frame CCD Frame number --- HJD-2448000 Heliocentric Date of Observation - 2448000 d V1 WIRO NW field phot. for star V1 mag V2 WIRO NW field phot. for star V2 mag V24 WIRO NW field phot. for star V24 mag V30 WIRO NW field phot. for star V30 mag V31 WIRO NW field phot. for star V31 mag V32 WIRO NW field phot. for star V32 mag V67 WIRO NW field phot. for star V67 mag V97 WIRO NW field phot. for star V97 mag Photometric parameters of M15 variables Vno Variable number --- Type RR Lyr Variable type --- Per Period d Ep-2448000 Epoch of maximum, offset JD 2448000 d u_Ep-2448000 Uncertainty flag on Ep-2448000 --- <V>int Intensity averaged V magnitude mag u_<V>int Uncertainty flag on <V>int number=1 One colon indicates photometric indices which are good, but not of the best quality; two colons (::) indicate photometric indices for variables with poor light curves or curves with large gaps. --- <V>mag Averaged V magnitude mag u_<V>mag Uncertainty flag on <V>mag number=1 One colon indicates photometric indices which are good, but not of the best quality; two colons (::) indicate photometric indices for variables with poor light curves or curves with large gaps. --- <V-R>int Intensity averaged V-R color mag u_<V-R>int Uncertainty flag on <V-R>int number=1 One colon indicates photometric indices which are good, but not of the best quality; two colons (::) indicate photometric indices for variables with poor light curves or curves with large gaps. --- <V-R>mag Averaged V-R color mag u_<V-R>mag Uncertainty flag on <V-R>mag number=1 One colon indicates photometric indices which are good, but not of the best quality; two colons (::) indicate photometric indices for variables with poor light curves or curves with large gaps. --- Radius Distance from cluster center arcsec Av Extinction in V band mag Ar Extinction in R band mag CDS 1996 Jul 26 * AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 27-Sep-1995 * Reformatted at CDS (F. Ochsenbein), and table6 added. J_AJ_110_704.xml A radio reference frame J/AJ/110/880 J/AJ/110/880 Radio reference frame A radio reference frame K J Johnston A L Fey N Zacharias J L Russell C Ma C de Vegt J E Reynolds D L Jauncey B A Archinal M S Carter T E Corbin M T Eubanks D R Florkowski D M Hall D D McCarthy P M McCulloch E A King G Nicolson D B Shaffer Astron. J. 110 880 1995 1995AJ....110..880J Positional data Radio sources VLBI A catalogue is presented based on the radio positions of 436 extragalactic sources distributed over the entire sky. The positional accuracy of the sources is better than 3 milliarcsec (mas) in both coordinates, with the majority of the sources having errors better than 1mas. This catalogue is based upon a general solution of all applicable dual frequency 2.3 and 8.4GHz Mark-III VLBI data available through the end of 1993 consisting of 1,015,292 pairs of group delay and phase delay rate observations. Details and positions are also given for an additional 124 objects that either need further observation or are currently unsuitable for the definition of a reference frame. The final orientation of the catalogue has been obtained by a rotation of the positions into the system of the International Earth Rotation Service and is consistent with the FK5 J2000.0 optical system, within the limits of the link accuracy.
Radio positions of sources used to define the reference frame Radio positions of candidate and other sources Class Source Classification number=1 1,2-defining; 3-candidate; 4,5-other; 6-not detected --- Name Source Name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s e_RAs Right ascension (J2000) Formal Error number=2 The formal errors refer to a position based on all observations of a source, which is different from the level of accuracy expected from only one observation or experiment. Systematic errors are estimated to be at the 0.5mas level. The right ascension formal error for 0420-014 was taken from the CTF solution because the right ascension of this source was fixed in the ICF solution to its a priori value in order to define the equinox. Consequently, the right ascension uncertainty of 0420-014 should be added in quadrature to the right ascension uncertainties of the remaining sources. s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec e_DEs Declination (J2000) Formal Error number=2 The formal errors refer to a position based on all observations of a source, which is different from the level of accuracy expected from only one observation or experiment. Systematic errors are estimated to be at the 0.5mas level. The right ascension formal error for 0420-014 was taken from the CTF solution because the right ascension of this source was fixed in the ICF solution to its a priori value in order to define the equinox. Consequently, the right ascension uncertainty of 0420-014 should be added in quadrature to the right ascension uncertainties of the remaining sources. arcsec Mean Mean Epoch of Observation (Epoch-1900) yr EpFirst Epoch of First Observation (Epoch-1900) yr EpLast Epoch of Last Observation (Epoch-1900) yr EpNexp Number of experiments in which a source was observed --- Nobs Number of delay/rate observations used in solution --- Sources observed unsuccessfully Class Source Classification number=1 1,2-defining; 3-candidate; 4,5-other; 6-not detected --- Name Source Name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Supplementary source identification Name Source name --- Type Optical identification number=1 QSO = quasar, BSO = blue stellar object, GAL = galaxy, LAC = BL Lac object, EF = empty field --- z Redshift --- mv Visual Magnitude mag S6cm 6cm (5GHz) Radio flux density Jy Alt Alternate name(s) --- Ref Reference --- CDS 1996 Jan 10 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 27-Sep-1995 J_AJ_110_880.xml The stellar initial mass function in the giant H II region NGC 595 J/AJ/111/1128 J/AJ/111/1128 UV-UBV photometry in NGC 595 The stellar initial mass function in the giant H II region NGC 595 E M Malumuth W H Waller J W Parker Astron. J. 111 1128 1996 1996AJ....111.1128M H II regions Photometry, UBV Photometry, ultraviolet As part of a larger effort to study the resolved and composite properties of the giant H II regions in Messier 33, we have analyzed multiband HST/WFPC-2 images of NGC 595 in terms of the ionizing cluster's resolved stellar population. Photometric reductions of the PC images yield 100 stars in the UV image, 272 stars on the U image, 345 stars on the B image, and 561 stars on the V image. A total of 267 stars are common to the U, B, and V images while 86 stars are detected on all 4 images. Although some clustering is evident, the degree of central concentration is less than that seen in 30 Doradus. The resulting U-B vs B-V diagram of the resolved stars is used to determine the reddening of each star. The average reddening derived from this diagram is E(B-V)=0.36+/-0.28mag. The dereddened color-M_V diagram is best fit by a model cluster having an age of 4.5+/-1.0Myr, and hence initial masses no greater than 51M_{sun}_. A total of 13 supergiant stars and 10 candidate WR stars [Drissen et al. (1993AJ....105.1400D), and references therein] are identified with M_V=-5 to -8mag. The remainder are main-sequence O-type (98) and early B-type (>145) stars with M_V=-1 to -6mag. The ratio of WR to O stars is WR/O=0.11+/-0.01, roughly the same as found in the core of 30 Doradus. The resulting luminosity function has a slope of alpha=-0.71. The derived IMF has a slope of Gamma=-1.32+/-0.02 before subtracting a background component, and Gamma=-1.00+/-0.05 after subtracting a background based on photometry of the surrounding WF images. Integration of the derived IMF down to a lower mass limit of 4M_{sun}_ yields a total mass of 7350M_{sun}_, while integration down to 0.1_{Msun}_ yields a total mass of 18000M_{sun}_. The total estimated ionizing luminosity is 5.0x10^50photon/s, roughly half that which is inferred from the Halpha luminosity in this region. This shortfall of ionizing photons can be reconciled by allowing for a spread in the stellar ages, and/or increasing the modeled EUV luminosity of the stars at the inferred cluster age.
NGC 595 photometry ID Identification number --- DMS Star number from table 1 of Drissen et al. (1993AJ....105.1400D) --- RAh Right ascension, J2000 h RAm Right ascension, J2000 min RAs Right ascension, J2000 s DE- Declination sign --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec UVmag Ultraviolet magnitude (F170W HST filter) mag Umag U magnitude mag Bmag B magnitude mag Vmag V magnitude mag CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 02-May-1996 J_AJ_111_1128.xml Membership of stars in NGC 1039 (M34) J/AJ/111/1193 J/AJ/111/1193 Proper motion in M34 Membership of stars in NGC 1039 (M34) B F Jones C F Prosser Astron. J. 111 1193 1996 1996AJ....111.1193J Clusters, open Photometry Proper motions We have measured proper motions, positions, magnitudes, and colors for 630 stars to V~16.2 in the vicinity of the open cluster NGC 1039=M34. A proper motion membership probability analysis has been performed. We give for all stars the equatorial coordinates, the proper motions, the V magnitude, and the membership probability. For the most likely cluster members we also give B-V and (V-I)K colors. Cross identifications with previous surveys are also provided. We find an age for the cluster of 200-250Myr and a distance of 475parsecs.
Positions and proper motions ID Identification number --- RAh Right ascension, Eq=1950 h RAm Right ascension, Eq=1950 min RAs Right ascension, Eq=1950 s DE- Declination sign --- DEd Declination, Eq=1950 deg DEm Declination, Eq=1950 arcmin DEs Declination, Eq=1950 arcsec pmX Proper motion, X 10-2arcsec/yr pmY Proper motion, Y 10-2arcsec/yr e_pmX Error in pmX 10-2arcsec/yr e_pmY Error in pmY 10-2arcsec/yr Vmag V magnitude mag B-V B-V color mag V-I V-I color mag Mem Membership probability % CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 02-May-1996 J_AJ_111_1193.xml A Proper-Motion Membership Study of the Old Open Cluster NGC 188 J/AJ/111/1205 J/AJ/111/1205 Proper-Motion Membership of Open Cluster NGC 188 A Proper-Motion Membership Study of the Old Open Cluster NGC 188 D I Dinescu T M Girard W F van Altena T Yang Y -W Lee Astron. Journ. 111 1205 1996 1996AJ....111.1205D Clusters, open Proper motions Relative proper motions have been determined for 1127 stars in the field of the open cluster NGC 188 from plates spanning a 60-year interval, taken with the 76-cm Thaw refractor of the Allegheny Observatory. Special attention has been paid to the corrections for systematic errors as a function of magnitude and color. The study is complete to a magnitude B = 16.2. Also some stars brighter than B = 12.5 were eliminated from the study because of the large uncertainty in estimating the magnitude equation at the bright end. The final relative proper motions have an accuracy of 0.5 mas/yr for well-exposed stars. From the cluster membership probabilities based on proper motions we obtain 360 cluster members, enabling us to better define the color-magnitude diagram. We provide a list of highly probable candidate blue stragglers in addition to the sample proposed by Eggen & Sandage (1969).
Master table ID identification number (AJ 111, 1205) --- IDUP identification number (Upgren at al. AJ 77, 74) --- IDS identification number (Sandage ApJ 135, 333) --- V V magnitudes (calibrated photographic magnitudes) mag B-V B-V colors mag X X coordinate mm Y Y coordinate mm RAh Right Ascension J2000 (h); mean epoch 1983.91 h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination sign --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (arcminutes) arcmin DEs Declination J2000 (arcseconds) arcsec pmX Proper Motion in X (milliarcseconds/yr) mas/yr pmY Proper Motion in Y mas/yr e_pmX Proper-motion error in X mas/yr e_pmY Proper-motion error in Y mas/yr Pc Proper-motion membership probability % Pcx Proper-motion and spatial (combined) membership probability % N Number of plates on which the object was measured --- Notes Explained at the end of the table 1 - photoelectric standards used in the photometric calibration (Sandage 77, 74) 2 - photometry from McClure and Twarog ApJ 214, 111 3 - photometry replaced from Caputo et al. AJ 99, 261 4 - stars with no magnitudes estimates from Lick plates which were used for the photometry 5 - stars with only V magnitudes from the Lick plates BS - blue stragglers (Eggen and Sandage ApJ 158, 669) ER Cep, ES Cep, V5, V8, V9 - short-period variables (Kaluzny and Shara ApJ 314, 585) --- Paul Kuin NASA/ADC 1997 May 19 J_AJ_111_1205.xml Binary star orbits from speckle interferometry. VIII. Orbits of 37 close visual systems J/AJ/111/370 J/AJ/111/370 Orbits of 37 close visual systems Binary star orbits from speckle interferometry. VIII. Orbits of 37 close visual systems W I Hartkopf B D Mason H A McAlister Astron. J. 111 370 1996 1996AJ....111..370H Interferometry Stars, double and multiple New orbital elements are presented for 37 close visual systems that have been observed and in some cases discovered by speckle interferometry. Periods of these systems range from 5.7 to 425yr, semimajor axes from 0.06" to 1.1". Four of these systems (Kui 18, Fin 325, StF 2597, and McA 77) had no previously published orbital analyses, while elements for a number of other systems have undergone major revisions. Finally, 135 new or revised interferometric measurements of these systems are also presented, as well as 8 negative results.
New speckle interferometric observations WDS WDS designation (epoch-2000 coordinates) WDS designation (epoch-2000 coordinates, in the manner of the Washington Double Star Catalogue <I/107> . --- Disc Binary star discoverer designation --- HD Henry Draper catalogue number --- Date Date of obs., as fractional Besselian year yr Theta Binary star position angle deg u_Theta Position angle uncertainty flag --- l_Rho Separation upper limit flag --- Rho Binary star separation arcsec u_Rho Separation uncertainty flag --- Lambda Filter effective wavelength nm n_Lambda + when two filters --- Lambda2 Second filter effective wavelength nm FWHM Filter FWHM nm Tel Telescope aperture The aperture sizes uniquely define the telescope used, as either the Cerro Tololo 4.0m, Kitt Peak 3.8m, Canada-France-Hawaii 3.6m, or Mount Wilson 2.5m telescope. m Notes Notes 1 = Re-reduction of archival data; secondary peak was originally either undetected or found too weak for reliable measurement. 2 = Re-reduction of an observation originally published by Hartkopf et al. (1994AJ....108.2299H) 3 = Re-analysis of the data originally published by McAlister et al. (1990AJ.....99..965M) found that the secondary peak was actually too close for reliable measurement. 4 = Previously unpublished negative result. --- CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 24-Feb-1996 J_AJ_111_370.xml ICCD Speckle observations of binary stars. XII. Measurements during 1984-1986 from the Perkins 1.8 m telescope J/AJ/111/393 J/AJ/111/393 Speckle observations of binary stars. XII ICCD Speckle observations of binary stars. XII. Measurements during 1984-1986 from the Perkins 1.8 m telescope A M Al-Shukri H A McAlister W I Hartkopf D J Hutter O G Franz Astron. J. 111 393 1996 1996AJ....111..393A I/107 : Washington Double Star Catalog (WDS) (Worley+ 1984) J/AJ/106/352 : ICCD speckle obs. of binary stars. VIII (Hartkopf+ 1993) J/AJ/106/637 : ICCD speckle obs. of binary stars. IX (Mason+, 1993) J/AJ/106/1639 : ICCD speckle obs. of binary stars. X (McAlister+ 1993) J/AJ/108/2299 : ICCD speckle obs. of binary stars. XI (Hartkopf+ 1994) J/AJ/111/936 : ICCD speckle obs. of binary stars. XIII (Hartkopf+ 1996) ftp://ftp.chara.gsu.edu/ : results from CHARA project Interferometry Stars, double and multiple Five hundred sixty-five measurements of 99 binary star systems are presented, obtained during 1984-1986 by means of speckle interferometry at the 1.8 m Perkins telescope on Anderson Mesa, Arizona. These observations were collected as part of a systematic program in which frequent speckle observations of nearby binary systems were to be used to attempt the detection of unseen companions through the analysis of residual motions in wide, visual binaries. This is the first of several papers in which these observations are presented and discussed.
Planet search observing list WDS WDS designation (epoch-2000 coordinates) WDS designation (epoch-2000 coordinates, in the manner of the Washington Double Star Catalogue <I/107>. --- GJ GJ number and components GJ number and components (from Gliese & Jahreiss, 1979, Third Catalogue of Nearby Stars (preliminary version), <V/70>) --- ADS Aitken Double Star designation Aitken Double Star designation (from Aitken, R.G. 1932, New General Catalogue of Double Stars Within 120 Degrees of the North Pole, (Carnegie Institution, Washington) --- Disc Binary star discoverer designation --- HD/DM HD or DM (BD, CD, or CPD) number --- Sp Spectral type --- V1 Visual magnitude of primary star mag V2 Visual magnitude of secondary star mag Rho Approximate binary separation arcsec Code Code for binary type Code for binary type: P = program star, C = comparison, S = standard --- Binary star speckle measures Name1 Star name 1, usually ADS or HR --- Name2 Star name 2, usually discoverer designation --- HD/DM HD or DM (BD, CD, or CPD) number --- SAO Smithsonian Astrophysical Observatory number --- WDS Washington Double Star Catalogue designation --- Date Date, as fractional Besselian year yr theta Position angle deg u_theta Position angle uncertainty flag --- rho Separation arcsec u_rho Separation uncertainty flag --- Obj Microscope objective and filter --- Qual Quality of measure, on a scale of 1 to 10 --- Patricia Bauer CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 27-Feb-1996 J_AJ_111_393.xml Distribution of blue galaxies in a merging cluster of galaxies Abell 168. J/AJ/111/42 J/AJ/111/42 Galaxies in Abell 168 Distribution of blue galaxies in a merging cluster of galaxies Abell 168. A Tomita F E Nakamura T Takata K Nakanishi T Takeuchi K Ohta T Yamada Astron. J. 111 42 1996 1996AJ....111...42T III/174 : Dressler's catalog of morphological types in 55 rich clusters of galaxies (1980ApJS...42..565D) Clusters, galaxy Galaxies, photometry V- and I- band CCD photometry of the central 0.18 square degree of Abell 168 was observed in November and December 1993 at the 1.05m Kiso Schmidt telescope (f/3.1). The CCD chip has 1000x1018 pixels, the pixel size is 0.752arcsec, giving a field of view of 12.0x12.7 arcmin. The total observed region was covered by 7 individual CCD fields. Note that some revisions were made by the author (TOMITA Akihiko) compared to the original publication.
Galaxies in Abell 168 ID Running number --- RAh Right Ascension 1950 (hours) number=1 The position accuracy is 5arcsec to 15arcsec depending on data quality. h RAm Right Ascension 1950 (minutes) number=1 The position accuracy is 5arcsec to 15arcsec depending on data quality. min RAs Right Ascension 1950 (seconds) number=1 The position accuracy is 5arcsec to 15arcsec depending on data quality. s DE- Declination 1950 (sign) number=1 The position accuracy is 5arcsec to 15arcsec depending on data quality. --- DEd Declination 1950 (degrees) number=1 The position accuracy is 5arcsec to 15arcsec depending on data quality. deg DEm Declination 1950 (minutes) number=1 The position accuracy is 5arcsec to 15arcsec depending on data quality. arcmin MajAxis Major axis diameter of the galaxy at 23 mag/arcsec2 isophote in I band arcsec Vmag V magnitude mag Imag I magnitude mag (V-I) color; it does not always coincide with (Vmag-Imag) because of round-off error. mag MType Eye inspected morphology number=2 category is either of E, S0, Se = early S [Sa-Sb], Sl = late S [Sc-Sd], I. If we can see any bar structure, we add `B'. --- Dressler Number given in Dressler =1980ApJS...42..565D --- HRV Heliocentric radial velocity taken from literature km/s Notes Various remarks, see number=3 We use the following abbreviations; LSB: low surface brightness; DBL: double system (the companion has the comparable size); COM: with a small companion (the number in parenthesis is the ID-number of the companion, if it is catalogued as another object in this list); comp: companion; dist: distortion; r: red; b: blue; sb: semi-blue; swb: somewhat blue. Note that No. 39 is the only IRAS source and No. 81 is the only radio source. -------------------------------------------------------------------------------- Remarks and Modifications: [TNT96] is used to designate the galaxies (ID column of table3) --- Francois Ochsenbein CDS 1996 Apr 12 Akihiko Tomita <atomita@milano.mtk.nao.ac.jp> J_AJ_111_42.xml A survey of Ca II H and K chromospheric emission in southern solar-type stars J/AJ/111/439 J/AJ/111/439 Chromospheric emission in late-type stars. A survey of Ca II H and K chromospheric emission in southern solar-type stars T J Henry D R Soderblom R A Donahue S L Baliunas Astron. J. 111 439 1996 1996AJ....111..439H Photometry Stars, atmospheres Stars, late-type More than 800 southern stars within 50pc have been observed for chromospheric emission in the cores of the Ca II H and K lines. Most of the sample targets were selected to be G dwarfs on the basis of colors and spectral types. The bimodal distribution in stellar activity first noted in a sample of northern stars by Vaughan and Preston (1980PASP...92..385V) is confirmed, and the percentage of active stars, about 30%, is remarkably consistent between the northern and southern surveys. This is especially compelling given that we have used an entirely different instrumental setup and stellar sample than used in the previous study. Comparisons to the Sun, a relatively inactive star, show that most nearby solar-type stars have a similar activity level, and presumably a similar age. We identify two additional subsamples of stars -- a very active group, and a very inactive group. The very active group may be made up of young stars near the Sun, accounting for only a few percent of the sample, and appears to be less than ~0.1Gyr old. Included in this high-activity tail of the distribution, however, is a subset of very close binaries of the RS CVn or W UMa types. The remaining members of this population may be undetected close binaries or very young single stars. The very inactive group of stars, contributing ~5%-10% to the total sample, may be those caught during a Maunder Minimum type phase. If the observations of the survey stars are considered to be a sequence of snapshots of the Sun during its life, we might expect that the Sun will spend about 10% of the remainder of its main sequence life in a Maunder Minimum phase.
Chromospheric activity observations HD Henry Draper number --- m_HD Component(s) of HD number --- Note Coded note 0 = target not listed in INCA (The Hipparcos Input Catalog) <I/196> 1 = double target listed as A and B in INCA, but components have different HD numbers 2 = target listed as AB in INCA, but split in this survey 3 = target listed as single in INCA, but with orbits in references B, D or G (see Ref below) * = note given at end of table --- Mult Multiplicity information Multiplicity information P = period in d(ays) or y(ears) s = separation in arcseconds a = semimajor axis of orbit in arcseconds --- Ref Coded reference for Mult Reference for multiplicity information B = Batten, Fletcher & MacCarthy 1989, Eighth Catalogue of the Orbital Elements of Spectroscopic Binary Systems, <V/64> D = Duquennoy & Mayor (1991A&A...248..485D) G = Gliese (1969VeARI..22....1G) (G69); Gliese & Jahreiss 1979, (1979A&AS...38..423G); 1991, Preliminary Version of the Third Catalog of Nearby Stars (GJ91) <V/70> H = Heintz (1984AJ.....89.1068H); (1994AJ....108.2338H) I = Hipparcos Input Catalog, Turon, C. et al. 1992, (INCA) <I/196> J = Jeffers, van den Bos & Greeby 1963, Index Catalogue of Visual Double Stars, 1961.0, Publications of the Lick Observatory, v. XXI (IDS). See WDS <I/107> W = Worley & Heintz 1983, Fourth Catalog of Orbits of Visual Binary Stars, <V/39> (WH83) --- Sample Coded sample information B = Best & Brightest C = Calibration N = Nearby P = Primary S = Secondary X = Extra --- Vmag V magnitude mag e_Vmag Error in Vmag mag B-V (B-V) color mag e_B-V Error in B-V mag MRef Coded reference for V and B-V Reference for magnitude and color information Ig = INCA, good data with (B-V) error <= 0.10 mag Ip = INCA, poor data with (B-V) error > 0.10 mag, only value available G = Gliese & Jahreiss 1991 <V/70> S = SIMBAD <http://cdsweb.u-strasbg.fr/Simbad.html> blank = no value available --- Date UT date of observation (ddmmyy) --- Flag Flag indicating special status of obs. Flag indicating special status of observation cal = calibration star con = contaminated spectrum hgh = very high SCTIO value (>0.600) low = very low SCTIO value (<0.180) noi = noisy spectrum off = minima of H and K lines out of dithering window pht = no (B-V) photometry available, or (B-V) out of sample range (0.50 to 1.00 for all samples) There are only 4 stars with (B-V)=0.40 to 0.49: 1 Primary, 1 Calibration, 2 Extra targets. ray = cosmic ray in necessary window spc = special target str = strange spectrum --- S(CTIO) S value from CTIO observation S is the flux index for the Ca II H and K lines --- S(MW) S value converted to Mt. Wilson system --- logR'(HK) Log R'(HK) value R'(HK) is the ratio of the emission from the chromosphere in the cores of the Ca II H and K lines to the total bolometric emission of the star. The prime denotes the substraction of a photospheric contribution to the observed H and K emission. --- Nobs Number of observations --- logR'(HK)m Mean log R' value of observations --- e_logR'(HK)m Error in logR'(HK)m --- Notes on individual objects in table 4 HD Star --- seq Line number when the note consists of several lines --- Text Text of note --- CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 07-Mar-1996 J_AJ_111_439.xml Optical Morphology of Bright Quasars on Images Taken With 1.2 m Schmidt Cameras J/AJ/111/645 J/AJ/111/645 Morphology of Quasars Optical Morphology of Bright Quasars on Images Taken With 1.2 m Schmidt Cameras D Fabian P D Usher Astron. J. 111 645 1996 1996AJ....111..645F II/207 : Palomar-Green catalog UV-excess stellar objects (Green+ 1986) QSOs The optical morphology of bright extragalactic objects listed by Green et al. (1986ApJS...61..305G) is determined on Palomar Observatory Sky Survey prints. Morphological types are assigned according to whether objects appear resolved or unresolved. These are plotted in the Hubble Diagram. When combined with previous results from the Medium-Bright Quasar Survey (MBQS), objects of redshift z are found to be unresolved on 1.2m Schmidt telescopes at apparent magnitudes brighter than B=21-3/4z over a large magnitude range 12.5<B<18.5. A luminosity cutoff for unresolved objects in this range is found to be M_B=-24, (H0=50), in agreement with an earlier estimate. Relevance to the search for large, bright, host galaxies, and for "naked quasar" candidates, is noted.
Morphology of objects listed by Green et al. (1986ApJS...61..305G, see cat. <II/207>) Object Coordinate-based object name --- EMor POSS E-print morphology The morphological designations of this paper are: G, galaxy; CG, compact galaxy (bright center and faint surrounding nebulosity); CGNN, a possible compact galaxy but with no nebulosity (a CG decided by shape); and *, starlike (an object indistinguishable from neighbouring stars). Any of these categories could be accompanied by the letter "C", meaning that the image is confused with another (usually fainter) source, while "?" connotes uncertainty. --- OMor POSS O-print morphology --- Note Note number in notes --- SpId Spectroscopic identification Spectroscopic identifications: QSO (quasar), Sey (Seyfert galaxy), BLL (BL Lacertae object), Gal (galaxy). --- Bmag B magnitude from Green et al., cat. <II/207> mag z Redshift Redshift from: Wampler & Ponz (1985ApJ...298..448W) Green et al. (1986ApJS...61..305G) Osterbrock & Pogge (1987ApJ...323..108O) Lipovetsky et al. (1988SoSAO..55....5L) --- Notes on individual objects in table 1 Note Note number If this field is blank, the data in field Text is a continuation from the previous record. --- Object Coordinate-based object name --- Text Text of the note --- table1.tex AASTeX version of table1.dat CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 07-Mar-1996 J_AJ_111_645.xml Seyfert galaxies with companions: orbital and kinematic clues to AGN triggering J/AJ/111/696 J/AJ/111/696 Rotation curves of Seyfert galaxies with companions Seyfert galaxies with companions: orbital and kinematic clues to AGN triggering W C Keel Astron. J. 111 696 1996 1996AJ....111..696K Galaxies, Seyfert Spectroscopy This paper presents imaging and optical spectroscopy of paired Seyfert galaxies and their companions. The aim is to seek common properties of Seyfert galaxies in interacting systems, which might provide evidence of AGN triggering in a way independent of the usual two-sample statistics which have proven ambiguous on this issue. Three kinds of comparison have been made -- the kinds of interactions involving Seyfert galaxies, the relative luminosities of the Seyferts and their companions, and the level of kinematic disturbance as measured from rotation curves. (1) Dynamics and tidal features have been used to determine (or at least limit) the sense of orbital motion (direct/ retrograde/polar with respect to the Seyfert galaxy's disk) for many of these pairs. There is no obviously preferred kind of interaction -- direct, polar, and retrograde encounters are all well represented, despite the gross differences in dynamical response of a disk to these various kinds of encounter. To the extent that triggering of Seyfert nuclei occurs due to tidal encounters, the existence of a perturbation seems more important than its exact duration or detailed effects on the disk. However, the ratio of merging to paired Seyferts is higher than for disk galaxies in general, consistent with more effective triggering of AGN in this specific phase; the implied time scale for enhanced occurrence during mergers is the same as the timescape for merger remnants to appear as such, a few disk-edge crossing times (typically several times 10^8yr). (2) Seyfert nuclei occur preferentially in the brighter members of galaxy pairs, by a median of 0.93mag after making the maximal correction for contaminating nonstellar light in the nuclei. Only about 1/3 of this effect can be accounted for by the known tendency of Seyfert nuclei to occur in more luminous galaxies. Enhancement of AGN by interactions is evidently more effective for more luminous galaxies (though this will also be the case if both star formation and AGN occurrence are enhanced in the same galaxies). (3) The rotation curves of the paired Seyferts show systematically small regions of rising or solid-body rotation compared to the disk radius, as a group comparable to Sa but very different from Sb or Sc galaxies (even for Seyfert galaxies with Hubble type later than Sa). There is weak evidence that this difference is also present with respect to more isolated Seyfert galaxies. Despite the obvious utility of a dynamically disturbed disk for transport of angular momentum and "feeding the monster," Seyfert galaxies in pairs actually have smaller kinematic disturbances (measured by the maximum departure from a symmetric rotation curve, normalized to the full rotation amplitude) than found in a complete sample of non-Seyfert spirals in pairs.
Rotation curve data Name Object name --- PA Position angle deg dHRV Correction to heliocentric velocity km/s Peak Pixel number of continuum peak pix Pixel Pixel number along the slit Pixel number along the slit, at a scale of 0.78 arcsec/pix. pix RVobs Mean radial velocity Mean radial velocity, in the observed frame and the so-called relativistic convention. km/s e_RVobs 2-sigma error derived from photon statistics km/s IHa Total H-alpha intensity (instrumental units) Total H-alpha intensity in instrumental units (neglecting the broad-line component where it can be distinguished). --- ICont Continuum intensity --- Nlines No. of emission lines measured at each point --- CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 08-Mar-1996 J_AJ_111_696.xml Faint Cepheid studies. I. Comparison with existing data sets J/AJ/111/902 J/AJ/111/902 Short-period Cepheids Faint Cepheid studies. I. Comparison with existing data sets A A Henden Astron. J. 111 902 1996 1996AJ....111..902H Photometry, UBVRI Stars, variable UBVRI data on 36 short-period (P<5days) Cepheids is given. The observing techniques and reduction procedures are described. A consistent set of finding charts, a set of standard stars for each Cepheid, and improved coordinates are also presented.
Comparison stars Name Comparison star name Name of comparison star: name of Cepheid plus a three-digit numeric suffix, e.g. v526_aql-001 --- GSC Guide Star Catalog number <II/143> --- RAh Right ascension, J2000 h RAm Right ascension, J2000 min RAs Right ascension, J2000 s DE- Declination sign, J2000 --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec Vmag V magnitude mag e_Vmag Error in Vmag mag B-V B-V color index mag e_B-V Error in B-V mag U-B U-B color index mag e_U-B Error in U-B mag V-R V-R color mag e_V-R Error in V-R mag R-I R-I color mag e_R-I Error in R-I mag Photometric data Name Variable star name Name of Cepheid variable star. If this field is blank, all other fields are continuations of the previous record. --- HJD-2440000 Heliocentric Julian Date - 2440000 d Vmag V magnitude mag B-V B-V color mag U-B U-B color mag V-R V-R color mag R-I R-I color mag Code Instrument system code Instrument system code, see table 1 of the printed paper. --- table3.tex AASTeX version of table3.dat table4.tex AASTeX version of table4.dat CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 02-May-1996 J_AJ_111_902.xml ICCD Speckle observations of binary stars. XIII. Measurements during 1989-1994 from the Cerro Tololo 4 m telescope J/AJ/111/936 J/AJ/111/936 ICCD Speckle obs. of binary stars. XIII ICCD Speckle observations of binary stars. XIII. Measurements during 1989-1994 from the Cerro Tololo 4 m telescope W I Hartkopf B D Mason H A McAlister N H Turner D J Barry O G Franz C M Prieto Astron. J. 111 936 1996 1996AJ....111..936H I/107 : Washington Double Star Catalog (WDS) (Worley+ 1984) J/AJ/106/352 : ICCD speckle obs. of binary stars. VIII (Hartkopf+ 1993) J/AJ/106/637 : ICCD speckle obs. of binary stars. IX (Mason+, 1993) J/AJ/106/1639 : ICCD speckle obs. of binary stars. X (McAlister+ 1993) J/AJ/108/2299 : ICCD speckle obs. of binary stars. XI (Hartkopf+ 1994) J/AJ/111/393 : ICCD speckle obs. of binary stars. XII (Al-Shukri+ 1996) ftp://ftp.chara.gsu.edu/ : results from CHARA project Interferometry Stars, double and multiple Nine hundred eighty-nine observations of 694 binary star systems, observed by means of speckle interferometry with the 4m telescope on Cerro Tololo, are presented. Included in these observations are three new interferometric binaries and new interferometric companions to four visual binaries. These measurements, made during the period 1989-1994, comprise the 13th installment of digital results stemming from our speckle program at several major observatories, and the 23rd list since the program's inception in 1975.
New interferometric components NameJ Epoch 2000 RA & Dec in manner of WDS --- DM Durchmusterung (BD, CD, or CP) number --- HD Henry Draper number --- CHARA Binary star discoverer (CHARA) designation --- Vmag Combined V magnitude mag dVmag V magnitude difference mag Sp Spectral type --- Epoch Discovery date, as fractional Besselian yr yr Sep Binary star separation, at discovery arcsec Period Estimated orbital period Estimated orbital period, assuming circular, face-on orbits with both components of equal brightness and mass yr Binary star speckle measurements WDS WDS number <I/107>, equinox 2000.0 The coordinates, which serve as the Washington Double Star Catalog (WDS) number, are for equinox 2000.0, but position angles have not been corrected for precession and are thus based upon the equinox for the epoch of observation (field Date). --- Disc Discoverer designation --- HD/DM Henry Draper or Durchmusterung number DM designations are BD numbers for declinations north of -21 deg, CPD numbers for stars further south. --- Date Observation date (-1900) yr Theta Position angle Accuracies are a function of stellar magnitude, magnitude difference, separation, and observing conditions; typical values for these observations are 1-3 mas in Rho and 0.1-0.2 deg in Theta. Colons following Theta or Rho values indicate measurements of somewhat reduced accuracy, usually the result of observing fainter systems or systems of larger magnitude difference. deg u_Theta Uncertainty flag for Theta --- Rho Angular separation arcsec u_Rho Uncertainty flag for Rho --- Lambda Filter effective wavelength and FWHM nm CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 10-Mar-1996 J_AJ_111_936.xml The horizontal branches of globular clusters. I. The color-magnitude diagram of NGC 6426 J/AJ/112/1054 J/AJ/112/1054 VI photometry of NGC 6426 The horizontal branches of globular clusters. I. The color-magnitude diagram of NGC 6426 R Zinn S Barnes Astron. J. 112 1054 1996 1996AJ....112.1054Z Clusters, globular Photometry Stars, horizontal branch A color-magnitude diagram of the globular cluster NGC 6426 has been constructed from photometry in the V and I passbands. The cluster has the steep giant branch indicative of a very metal-poor composition. Following the technique of Sarajedini (1994AJ....107..618S), we derive [Fe/H]=-2.31+/-0.10 and E(V-I)=0.54+/-0.03 [E(B-V)=0.40+/-0.02] from a comparison with the giant branches of other globular clusters. These values are very close to the ones obtained from photometry of the cluster's integrated light, and the weighted means of our results and the previous ones are [Fe/H]=-2.28+/-0.09 and E(B-V)=0.41+/-0.02. The mean V magnitude of the horizontal branch (HB) at the instability strip is 18.12+/-0.05, from which we estimate that NGC 6426 lies 17.4kpc from the Sun, 11.5kpc from the galactic center, and 4.9kpc from the galactic plane. NGC 6426 resembles NGC 5466 and M68 in both [Fe/H] and HB morphology. The HB of NGC 6426 overlaps the one in M15 from the red HB to M15's gap in the blue HB, but there is no evidence of significant numbers of faint blue HB stars in NGC 6426 that are analogous to the ones constituting the "extended HB" in M15.
NGC 6426 17 44.9 +03 11
Photometry of NGC 6426 Star Star number in cluster --- Xpos X coordinate on the master frame number=1 The origin of the pixel numbers is at lower left corner. North is at the left, and east is at the bottom. pix Ypos Y coordinate on the master frame number=1 The origin of the pixel numbers is at lower left corner. North is at the left, and east is at the bottom. pix Vmag V magnitude mag e_Vmag Error in V as given by DAOPHOT mag V-I V-I color index mag e_V-I Error in V-I as given by DAOPHOT mag CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 25-Sep-1996 J_AJ_112_1054.xml Luminosity functions for post-turnoff stars in globular clusters. II. NGC 7099 J/AJ/112/1061 J/AJ/112/1061 BV photometry of NGC 7099 Luminosity functions for post-turnoff stars in globular clusters. II. NGC 7099 P A Bergbusch Astron. J. 112 1061 1996 1996AJ....112.1061B Clusters, globular Photometry, CCD Stars, bright New BV CCD photometry for the bright stars in cluster fields centered on the core of NGC 7099 is presented. The morphology of the LF though the turnoff region is similar to that found in other metal-poor clusters in that the relative number of turnoff to giant stars is lower than predicted by canonical models. Comparisons with evolutionary sequences of horizontal branch stars suggest a reddening E(B-V)=0.06 and a distance modulus (m-M)_V=14.83. Isochrone fits to [Fe/H]=-2.03, [O/Fe]=+0.70 models are consistent with an age of at least 14 Gyr. The model LF for this age accurately predicts the brightness of the tip of the red giant branch (RGB) as well as the location of the break which signals the transition from the base of the RGB to the main sequence. There is an indication that the evolutionary pause on the RGB, which manifests itself as a bump in the LF, occurs one magnitude fainter than the models predict. The excess of HB stars with respect to giants is confirmed and implies a helium abundance Y=0.28, which is higher than that found in other metal-poor globular clusters from the R method. From a comparison with the metal-rich, blue horizontal branch cluster NGC 288, it is argued that age cannot by itself be the solution to the second parameter problem.
NGC 7099 21 40.3 -23 11
Photometry for stars brighter than V=18.0 Star Star number --- Xpos X pixel coordinate pix Ypos Y pixel coordinate pix Vmag V magnitude mag B-V B-V color index mag Chi Mean profile fitting statistic, chi --- CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 25-Sep-1996 J_AJ_112_1061.xml Additional emission-line candidates from the HK survey J/AJ/112/1188 J/AJ/112/1188 HK survey emission-line candidates Additional emission-line candidates from the HK survey T C Beers S Rossi D Ulrich R Wilhelm Astron. J. 112 1188 1996 1996AJ....112.1188B J/AJ/108/268 : HK survey emission-line candidates positions (Beers+ 1994) J/ApJS/76/1001 : UBV photometry of HK survey stars (Preston+, 1991) J/PASP/102/1392 : UBV photometry from HK survey. I (Doinidis+ 1990) J/PASP/103/973 : Photoelectric UBV from HK survey. II (Doidinis+ 1991) Positional data Stars, emission We present a list of 218 additional candidate emission-line objects discovered with the northern and southern HK interference-filter/ objective-prism survey of Beers and collaborators. The objects have apparent magnitudes in the range 10<=B<=16, several magnitudes fainter than obtained with previous prism surveys of similar resolution. Of the new candidates, 73 have been previously identified. The total list of HK-survey emission-line candidates now numbers 376 objects, 104 of which were noted by previous surveys.
Emission-line candidates from the HK survey Star Plate and star number --- n_Star Note if previous identification Asterisk, "*", if present indicates a previous identification is available. More information about previous identifications can be found in Table 2 of the printed paper (not included here) --- BrCode Brightness classification code vb: very bright b: bright mb: medium bright m: medium mf: medium faint f: faint vf: very faint --- RAh Right Ascension, epoch 2000.0 h RAm Right Ascension, epoch 2000.0 min RAs Right Ascension, epoch 2000.0 s DE- Declination sign --- DEd Declination, epoch 2000.0 deg DEm Declination, epoch 2000.0 arcmin DEs Declination, epoch 2000.0 arcsec GLON Galactic longitude deg GLAt Galactic latitude deg Comment Comments on the emission detected Description of the nature of the detected emission are in three broad groups: weak (wk), moderate (mod), and strong (str), corresponding to the strength of the emission feature relative to the surrounding continuum. Spectra with emission apparent in the cores of the Ca II H and K absorption features are noted as "core" emission objects. Spectra with variable emission lines, which means the strength of the emission appeared to vary across the 90-minute exposure, are noted as "var". Balmer emission refers to emission lines detected at the location of the H-8 Balmer line, which is just visible at the blue edge of the spectra, and occasionally, for exceptionally strong emission, even in the Halpha line, which is redward of the nominal filter cutoff. Objects with emission which did not appear to fall at the location of the Ca II HK features, or Balmer features are noted as "others." --- CDS 1997 Jan 31 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 09-Oct-1996 J_AJ_112_1188.xml A high-resolution catalog of cometary emission lines J/AJ/112/1197 J/AJ/112/1197 Catalog of cometary emission lines A high-resolution catalog of cometary emission lines M E Brown A H Bouchez H Spinrad C M Johns-Krull Astron. J. 112 1197 1996 1996AJ....112.1197B Comets Spectroscopy Using high-resolution spectra obtained with the Hamilton echelle spectrograph at Lick Observatory, we have constructed a catalog of emission lines observed in comets Swift-Tuttle and Brorsen-Metcalf. The spectra cover the range between 3800A and 9900A with a spectral resolution of {lambda}/{DELTA}{lambda}~42000. In the spectra, we catalog 2997 emission lines of which we identify 2438. We find cometary lines due to H, O, C2, CN, NH2, C3, H2O+, CH, and CH+. We list 559 unidentified lines compiled from the two spectra and comment on possibilities for their origins.
Catalog of emission lines LamST Wavelength for line from Swift-Tuttle 0.1nm n_LamST Flag for blend with previous line A "+" in this column indicates that the line with the wavelength listed in the previous row has been identified as a blend of two or more lines, with the laboratory wavelengths and identifications given in the subsequent rows. --- IntST Relative intensity of Swift-Tuttle line These intensities are corrected for the echelle blaze function, but not for CCD response or atmospheric absorption. The relative intensities are thus reliable within a spectral order but not between widely spaced orders. --- LamBM Wavelength, line from Brorsen-Metcalf 0.1nm n_LamBM Flag for blend with previous line --- IntBM Rel. intensity of Brorsen-Metcalf line --- LamLab Laboratory wavelength of identified line 0.1nm Species Identified molecule or 'unid.' --- Band Identified band or blank --- Trans Identified transition, or blank --- CDS 1997 Jan 31 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 09-Oct-1996 J_AJ_112_1197.xml The Hubble Deep Field observations, data reduction, and galaxy photometry. J/AJ/112/1335 J/AJ/112/1335 Hubble Deep Field observations The Hubble Deep Field observations, data reduction, and galaxy photometry. R E Williams B Blacker M Dickinson W van Dyke Dixon H C Ferguson A S Fruchter M Giavalisco R L Gilliland I Heyer R Katsanis Z Levay R A Lucas D B McElroy L Petro M Postman H -M Adorf R N Hook Astron. J. 112 1335 1996 1996AJ....112.1335W J/AJ/112/359 : Galaxies in the Hubble Deep Field (van den Bergh+ 1996) J/ApJ/453/48 : VI photometry of HST faint field galaxies (Driver+ 1995) Galaxies, photometry The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.
HST
Hubble Deep Field source catalog ID Identification number --- Xpos X position number=1 1 pix = 0.1 arcsec; x increasing from left to right, y increasing from low to top pix Ypos Y position number=1 1 pix = 0.1 arcsec; x increasing from left to right, y increasing from low to top pix RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec l_mt Limit flag on mt --- mt Total magnitude mag l_mi Limit flag on mi --- mi Isophotal magnitude mag l_U-B Limit flag on U-B --- U-B U-B colour index mag l_B-V Limit flag on B-V --- B-V B-V colour index mag l_V-I Limit flag on V-I --- V-I V-I colour index mag S/N Signal-to-noise ratio --- area Area arcsec2 r1 Unweighted first moment radius arcsec b/a Ellipticity --- PA Position angle deg Flag Flags --- table7.ps PostScript version of table7 tables.fit FITS tables of the complete set of parameters for each galaxy Francois Ochsenbein CDS 1996 Nov 27 Copied on 27-Nov-1996 via FTP from http://www.stsci.edu/ftp/observer/hdf/archive/v2catalog J_AJ_112_1335.xml A spectroscopic survey for binary stars in the globular cluster NGC 5053. J/AJ/112/1489 J/AJ/112/1489 Spectroscopic survey for binaries in NGC 5053 A spectroscopic survey for binary stars in the globular cluster NGC 5053. L Yan J G Cohen Astron. J. 112 1489 1996 1996AJ....112.1489Y Binaries, spectroscopic Clusters, globular Radial velocities We carried our a radial velocity survey for spectroscopic binaries in the low-density globular cluster NGC 5053. Our sample contains a total of 77 cluster member giant and subgiant stars with visual magnitudes of 14.5-18.6. Of These 77 stars, 66 stars have on average of 3-4 measurements with a total of 236 velocities. A typical velocity error per measurement is 13km/s. The stars in our sample are spatially distributed from the cluster center out to 10arcmin in radius (4.5 core radii). Among theses 66 stars with multiple velocity measurements, we discovered 6 spectroscopic binary candidates.
Relative radial velocities of stars in NGC 5053 (individual data) Star Star identification name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Dist Radial distance from the cluster arcsec HJD Heliocentric Julian date of observation d HRV Heliocentric radial velocity km/s e_HRV rms uncertainty on HRV km/s Relative radial velocities of stars in NGC 5053 (average data) Star Star identification name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Dist Radial distance from the cluster arcsec n_VR Number of observations --- VR Weighted mean radial velocity number=1 When n_VR=1, only one measurement km/s e_VR External velocity error in a single measurement estimated from the dispersion about the mean km/s chi2 Radial velocity variability over the timespan of three years --- P(<chi2) Probability number=2 To evaluate the significance of the variations represented by chi2, we calculated the probability P(<chi2) of having a chi2 at least this large purely due to chance fluctuations with a Gamma function Q(0.5{nu}, 0.5chi2), here {nu} is the number of the degree of freedom. Reasonable limits of chi2 probability for identifying significant variations are 0.01-0.001. --- V0 Deredenned V magnitude number=3 Photmetry for stars beginning by S is from Sandage et al. (1977AJ.....82..389S) mag (B-V)0 Deredenned B-V colour index number=3 Photmetry for stars beginning by S is from Sandage et al. (1977AJ.....82..389S) mag table2.tex TeX version of table 2 Patricia Bauer CDS 1997 Nov 17 Lin Yan <lyan@eso.org> J_AJ_112_1489.xml K Giants in Baade's Window. II. The Abundance Distribution J/AJ/112/171 J/AJ/112/171 K Giants in Baade's Window. II K Giants in Baade's Window. II. The Abundance Distribution E M Sadler R M Rich D M Terndrup Astron. J. 112 171 1996 1996AJ....112..171S J/AJ/110/1774 : K giants in Baade's window. I. (Terndrup+ 1995) Abundances, [Fe/H] Effective temperatures Magnitudes Stars, giant This is the second in a series of papers in which we analyze spectra of over 400 K and M giants in Baade's Window, including most of the stars with proper motions measured by Spaenhauer et al. (1992AJ....103..297S). In our first paper, we measured line-strength indices of Fe, Mg, CN, and HBeta and calibrated them on the system of Faber et al. (1985ApJS...57..711F). Here, we use the <Fe> index to derive an abundance distribution of [Fe/H] for 322 stars with effective temperatures between 3900K and 5160K. Our derived values of [Fe/H] agree well with those measured from high-resolution echelle spectra (e.g., McWilliam & Rich, 1994ApJS...91..749M) for the small number of stars in common. We find a mean abundance <[Fe/H]>=-0.11+/-0.04 for our sample of Baade's Window K giants. More than half the sample lie in the range -0.4<[Fe/H]<+0.3. We estimate line-of-sight distances for individual stars in our sample and confirm that, in Baade's Window, most K giants with V<15.5 are foreground disk stars, but the great majority (more than 80%) with V>16 belong to the bulge. We also compare the metallicities derived from the CN and Mg2 indices to those from iron. Most of the metal-rich stars in our sample appear to be CN-weak, in contrast to the situation in metal-rich globular clusters and elliptical galaxies. The metal-poor half of our sample ([Fe/H]<0) shows evidence for a mild Mg overenhancement ([Mg/Fe]~+0.2); but this is not seen in the more metal-rich stars ([Fe/H]>=0). The K giants in Baade's Window therefore share some, but not all, of the characteristics of stars in elliptical galaxies as inferred from their integrated light.
Measurements of [Fe/H] for Baade's Window K giants Star Star name --- Vmag V magnitude mag V-I V-I color mag Teff Effective temperature K [Fe/H] Metallicity, [Fe/H] Sun e_[Fe/H] Error in [Fe/H] --- R Distance kpc e_R Error in R kpc Class Star classification C = bulge clump/RGB B = bulge giant branch D = disk giant branch H = halo giant --- table1.tex AASTeX version of table1.dat CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 09-Oct-1996 J_AJ_112_171.xml Large-Scale Structure at Low Galactic Latitude J/AJ/112/1803 J/AJ/112/1803 Large Scale Structure Large-Scale Structure at Low Galactic Latitude R O Marzke J P Huchra M J Geller Astron. J. 112 1803 1996 1996AJ....112.1803M VII/193 : The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995) Clusters, galaxy We have extended the CfA Redshift Survey to low galactic latitudes to investigate the relation between the Great Wall in the North Galactic Cap and the Perseus-Pisces chain in the South Galactic Cap. We present redshifts for 2020 galaxies in the Catalogue of Galaxies and of Clusters of Galaxies (Zwicky et al. 1961-68, CGCG, Cat. <VII/4>) in the following regions: 4h<=RA<=8h, 17h<=Dec.<=20h, 0deg<=Dec.<=45deg. In these regions, the redshift catalogue includes 1664 galaxies with B(0)<=15.5 (of which 820 are newly measured) and is 97% complete. We also include redshifts for an additional 356 galaxies in these regions with B(0)>15.5; of these, 148 were previously unmeasured. The CGCG samples the galaxy distribution down to b_(II)_~10deg. In this paper, we discuss the acquisition and reduction of the spectra, and we examine the qualitative features of the redshift distribution. The Great Wall and the Perseus-Pisces chain are not simply connected across the Zone of Avoidance. These structures, which at first appear to be coherent on scales of ~100h^-1^Mpc or more, actually form the boundaries of neighboring voids of considerably smaller scale, approximately 50h^-1^Mpc. The structures delineated by our optically-selected sample are qualitatively similar to those detected by the far-infrared-selected IRAS 1.2 Jansky Survey (Fisher et al., 1995ApJS..100...69F). Although the IRAS survey probes more deeply into the Zone of Avoidance, our optically-selected survey provides better sampling of structures at b_(II)>=10deg. (Copyright) 1996 American Astronomical Society.
The Galactic Plane Survey [B(0)<=15.5] The Galactic Plane Survey [B(0)>=15.5] Name Source name --- RAh Right Ascension (1950) h --- Always ':' --- RAm Right Ascension (1950) min --- Always ':' --- RAs Right Ascension (1950) s DE- Sign, Declination --- DEd Declination (1950) deg --- Always ':' --- DEm Declination (1950) arcmin --- Always ':' --- DEs Declination (1950) arcsec m(zw) Zwicky B(0) magnitude mag r_m(zw) Source code for m(zw) (if not from CGCG) Source code for magnitude if not from CGCG. "H" refers to magnitudes split by eye by JPH; "K" refers to magnitudes from Kirshner et al. (1978, Cat. <J/AJ/83/1549>; 1983, <J/AJ/88/1285>). --- HRV Heliocentric radial velocity, cz km/s e_HRV Error in HRV km/s Source Redshift source code (see table3.dat) --- Morph Morphological type Morphological types are de Vaucouleurs' T types from the RC2, Uppsala Catalog and the Revised Shapley-Ames Catalog. Some additional types have been defined for peculiar and untyped objects and for objects that are in catalogues of extragalactic objects but are really galactic in nature. Additional types for galaxies in the CfA Redshift Survey region (described below) have been estimated by J. Huchra from glass copies of the Palomar Sky Survey. Types for southern galaxies come from both the ESO catalog and the Vorontsov-Velyaminov Catalogs. Morphological types codes are: -7 Elliptical (Unclassified) -6 Compact Elliptical -5 E, and dwarf E -4 E/S0 -3 L-, SO- -2 L, SO -1 L+, SO+ 0 SO/a, SO-a 1 Sa 2 Sab 3 Sb 4 Sbc 5 Sc 6 Scd 7 Sd 8 Sdm 9 Sm, Magellanic Spiral 10 Im, Irr I, Magellanic Irregular, Dwarf Irregular 11 Compact Irregular, Extragalactic HII Region 15 Peculiar, Unclassifiable 16 Irr II 20 S..., Sc-Irr, Unclassified Spiral 25 Plate Flaw, Star, etc. misclassified as galaxy 33 Reflection Nebula, misclassified as galaxy 32 HII Region misclassified as galaxy 30 Planetary Nebula, misclassified as galaxy 40 Part of a galaxy, e.g. a bright HII region like N5471 --- Bar Bar type A unbarred X mixed type B barred --- Lum Luminosity class Luminosity Classes (for Spirals and Irregulars) 1 I 6 III-IV 2 I-II 7 IV 3 II 8 IV-V 4 II-III 9 V 5 III --- Pec Peculiarities P = Peculiar S = No inner ring R = Ringed (outer) T = Pseudo inner ring D = Double or Multiple --- D1 Major axis diameter arcmin D2 Minor axis diameter arcmin UGC UGC (Cat. VII/26>) number --- Comments Comments & references to other catalogues If the comment is "See Notes," then there is a note about a superposed star in the corresponding notes file. --- Notes to table1.dat Notes to table2.dat Name Source name --- Note Superposed star(s) name(s) or other note --- Velocity sources Source Redshift source code --- Reference Reference to redshift source --- CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 30-Mar-1997 J_AJ_112_1803.xml Multicolor CCD photometry of the SMC cluster Kron 3 J/AJ/112/2004 J/AJ/112/2004 CCD photometry of SMC cluster Kron 3 Multicolor CCD photometry of the SMC cluster Kron 3 G Alcaino W Liller F Alvarado V Kravtsov A Ipatov N Samus O Smirnov Astron. J. 112 2004 1996 1996AJ....112.2004A Clusters, open Photometry, CCD We present BVRI CCD photometry of 3149 stars in the SMC populous cluster Kron 3. Radial dependence of the horizontal branch morphology has been revealed. Contrary to Rich et al. (1984ApJ...286..517R), we conclude that the cluster radius is about r=6'. We estimate the cluster metallicity as [Fe/H]=-1.26 and its apparent distance modulus as (m-M)=18.75mag. Our estimate of the cluster age, based on fitting isochrones of VandenBerg & Bell (1985ApJS...58..561V) to our V-(B-V) and V-(V-R) diagrams, is about 10Gyr, the lower limit being 8Gyr; this values is greater than those derived earlier, presumably partially due to the distance modulus values used by earlier investigators being too large. Our age estimate is not far from the upper values from Righ et al. (1984ApJ...286..517R).
Kron 3 Lindsay 8 00 24 46.3 -72 47 37
CCD photometry in Kron 3 Seq Running number --- Xpos x coordinate (along RA, increases to the east) pix Ypos y coordinate (along DE, increases to the north) pix Vmag V magnitude mag B-V B-V color index mag V-R V-R color index mag V-I V-I color index this column in the printed paper is inadvertently labelled "R-I". mag Francois Ochsenbein CDS 1996 Dec 16 It is a pleasure to thank Prof. Nikolai N. Samus <samus@sai.msu.su> for providing a copy of Table3 to CDS. J_AJ_112_2004.xml Prospects for determining asteroid masses J/AJ/112/2319 J/AJ/112/2319 Asteroid masses Prospects for determining asteroid masses J L Hilton P K Seidelmann J Middour Astron. J. 112 2319 1996 1996AJ....112.2319H Minor planets The orbits of 4583 main belt asteroids are integrated orbits for 57 years and searched for asteroid-asteroid encounters from which it may be possible to determine the masses of 23 of the largest asteroids (diameter>=200km) and 11 smaller asteroids. The search is conducted using a scattering formula which serves as a useful filter for identifying encounters that can lead to a mass determination. A total of 460 such encounters were found. The ten most useful of these encounters are examined in detail. The results show that, to make a reliable mass determination, the mean distance of the perturbed asteroid must be known to within a few times 10^-8^AU. An observing program targeting the asteroids listed here would have a substantial impact on our knowledge of asteroid masses and densities.
Significant encounters involving large asteroids Date Date of least separation "DD/MM/YYYY" Larger Name of larger asteroid --- LType Tholen et al. (1989) type of Larger First letter of the classification from Tholen, D. J. 1989, in Asteroids II, edited by R. P. Binzel, T. Gehrels, & M. S. Matthews, (University of Arizona Press, Tucson) p. 1139. --- Smaller Name of smaller asteroid --- SType Tholen et al. (1989) type of Smaller --- Dist Distance between on Date at 0 hr. UT AU Time Number of days distance less than 0.05 AU d Qual Quality factor, from 1 to 5 The quality factor is an estimate of the likelihood of producing a useful mass from the encounter. The quality factor runs from 1 (low probability of significant deflection) to 5 (high probability) and is computed as the logarithm of the computed deflection angle in arc seconds, rounded to the nearest integer. --- table2.tex AASTeX version of table2 CDS 1997 Jan 31 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 05-Nov-1996 J_AJ_112_2319.xml BVRI Light Curves for 29 Type Ia Supernovae J/AJ/112/2408 J/AJ/112/2408 Light Curves of 29 SNe BVRI Light Curves for 29 Type Ia Supernovae M Hamuy M M Phillips N B Suntzeff R A Schommer J Maza R Antezana M Wischnjewsky G Valladares C Muena L E Gonzales R Aviles L A Wells R C Smith M Navarrete R Covarrubias G M Williger A R Walker A C Layden J H Elias J A Baldwin M Hernandez H Tirado P Ugarte R Elston N Saavedra F Barrientos E Costa P Lira M T Ruiz C Anguita X Gomez P Ortiz M Della Valle J Danziger J Storm Y -C Kim C Bailyn E P Rubenstein D Tucker S Cersosimo R A Mendez L Siciliano W Sherry B Chaboyer R A Koopmann D Geisler A Sarajedini A Dey N Tyson R M Rich R Gal R Lamontagne N Caldwell P Guhathakurta A C Phillips P Szkody C Prosser L C Ho R McMahan G Baggley K -P Cheng R Havlen K Wakamatsu K Janes M Malkan F Baganoff P Seitzer M Shara C Sturch J Hesser P Hartigan J Hughes D Welch T B Williams H Ferguson P J Francis L French M Bolte J Roth S Odewahn S Howell W Krzeminski Astron. J. 112 2408 1996 1996AJ....112.2408H Photometry Supernovae BV(RI)_KC_ (see Bessel, 1990PASP..102.1181B) light curves are presented for 27 type Ia supernovae discovered during the course of the Calan/Tololo Survey and for two other SNe Ia observed during the same period. Estimates of the maximum light magnitudes in the B, V, and I bands and the initial decline rate parameter {DELTA}m_(15)(B) are also given. (Copyright) 1996 American Astronomical Society.
BV(RI)_KC_ photometry for the 29 SNe Ia SN Supernova designation --- HJD Julian Date of Observation d Bmag B magnitude mag e_Bmag Error in Bmag The uncertainties quoted for each magnitude correspond to the sum in quadrature of the errors due to photon Poisson statistics and an _assumed_ additional error of 0.03mag in each individual observation. The latter uncertainty was included in order to account for errors involved in the transformation from the authors' instrumental system to the standard system, and also due to the subtraction of the underlying host galaxy. mag Vmag V magnitude mag e_Vmag Error in Vmag mag Rmag R magnitude mag e_Rmag Error in Rmag mag Imag I magnitude mag e_Imag Error in Imag mag CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 30-Mar-1997 J_AJ_112_2408.xml The Ursa Major cluster of galaxies. I. Cluster definition and photometric data J/AJ/112/2471 J/AJ/112/2471 The Ursa Major cluster. I. The Ursa Major cluster of galaxies. I. Cluster definition and photometric data R B Tully M A W Verheijen M J Pierce J -S Huang R J Wainscoat Astron. J. 112 2471 1996 1996AJ....112.2471T Galaxies, photometry Photometry, CCD Photometry, surface The Ursa Major Cluster has received remarkably little attention, although it is as near as the Virgo Cluster and contains a comparable number of H I-rich galaxies. In this paper, criteria for group membership are discussed and data are presented for 79 galaxies identified with the group. Of these, all 79 have been imaged at B,R,I bands with CCDs, 70 have been imaged at K' with a HgCdTe array detector, and 70 have been detected in the H I 21 cm line. A complete sample of 62 galaxies brighter than M_B=-16.5 is identified. Images and gradients in surface brightness and color are presented at a common linear scale. As has been seen previously, the galaxies with the reddest global colors are reddest at the centers and get bluer at large radii. However, curiously, among the galaxies with the bluest global colors there are systems with very blue cores that get redder at large radii.
Cluster members PGC Principal Galaxies Catalogue <VII/119> name Decimal extensions given to objects without PGC names --- Name Alternate name Alternate name; order of preference: NGC, UGC or name built from RA and dec. Note: 1148+48 = Mkn 1460; 1156+46 = UGCA 259 --- Flag Flag for faintness or membership f: galaxies fainter than complete sample limit q: questioned membership --- RAh Right ascension, 1950 h RAm Right ascension, 1950 min RAs Right ascension, 1950 s DE- Declination sign, always blank --- DEd Declination, 1950 deg DEm Declination, 1950 arcmin DEs Declination, 1950 arcsec GLON Galactic longitude deg GLAT Galactic latitude deg SGL Supergalactic longitude deg SGB Supergalactic latitude deg Type Numeric type code --- AB Galactic absorption in B band mag Vhel Heliocentric velocity km/s V0 Vhel + 300sin(l)cos(b) km/s e_Vhel Uncertainty in Vhel km/s W20 Linewidth at 20% of peak flux km/s e_W20 Uncertainty in W20 km/s Flux HI line flux Jy.km/s Raw photometric data PGC Principal Galaxies Catalogue <VII/119> name --- Type Numeric type code --- Name NGC, UGC, or coordinate name --- PA Position angle (east from north) deg Ecc Eccentricity (1-(b/a)) --- R(B25) Radius at isophotal level of 25mag/arcsec2 in B arcsec Filter Filter --- Date Date of observation "DD/MM/YY" BIso Raw B magnitude above 27 mag/arcsec^2^ mag BTot Raw B magnitude extrapolated to infinity mag mu4 Surface brightness within 4" ellipse of center mag/arcsec2 mu0 Extrapolated disk central surface brightness mag/arcsec2 h Exponential disk scale length arcsec R20% Radius enclosing 20% of total light arcsec R50% Radius enclosing 50% of total light arcsec R80% Radius enclosing 80% of total light arcsec Reduced photometric data PGC Principal Galaxies Catalogue <VII/119> name --- Name NGC, UGC, or coordinate name --- Type Numeric type code --- BTbi Total B magnitude adjusted for galactic and inclination-dependent obscuration mag RTbi Total R magnitude adjusted for obscuration mag ITbi Total I magnitude adjusted for obscuration mag K'Tbi Total K' magnitude adjusted for obscur. mag B-R B-R color, adjusted for obscuration mag B-I B-I color, adjusted for obscuration mag B-K' B-K' color, adjusted for obscuration mag hR/hB Ratio of R and B scale lengths --- hI/hB Ratio of I and B scale lengths --- hK/hB Ratio of K' and B scale lengths --- <C82> Concentration index: ratio of radii containing 80% and 20% of the total light --- logLB log luminosity in B; solar units solLum Incl Inclination from face-on deg MBbi Absolute B magnitude; m-M=30.95 mag MRbi Absolute R magnitude; m-M=30.95 mag MIbi Absolute I magnitude; m-M=30.95 mag MKbi Absolute K' magnitude; m-M=30.95 mag mu0(B-R) Differential B-R central disk surface brightness mag/arcsec2 mu0(B-I) Differential B-I central disk surface brightness mag/arcsec2 mu0(B-K) Differential B-K' central disk surface brightness mag/arcsec2 Bmu0-mu4 Differential surface brightness in B Differential surface brightness of central disk minus mean surface brightness within 4" ellipse in the band considered. mag/arcsec2 Rmu0-mu4 Differential surface brightness in R mag/arcsec2 Imu0-mu4 Differential surface brightness in I mag/arcsec2 Kmu0-mu4 Differential surface brightness in K mag/arcsec2 logLK log luminosity in K' solLum CDS 1997 Nov 26 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 06-Nov-1996 NOTICE: the published version of Table2 differs from the CD-ROM version. * 26-Nov-1997: a corrected version of table2 was introduced at CDS, supplied by Marion Schmitz (zb4ms@ipac.caltech.edu) J_AJ_112_2471.xml Near infrared JHK photometry of intermediate redshift clusters J/AJ/112/2500 J/AJ/112/2500 JHK' photometry of 4 clusters of galaxies Near infrared JHK photometry of intermediate redshift clusters I S McLean H Teplitz Astron. J. 112 2500 1996 1996AJ....112.2500M Clusters, galaxy Photometry, infrared Deep near-infrared images of four intermediate redshift (z=0.2-0.4) clusters (Abell 370, Abell 963, CL 0024+1654 and CL 0909+4408) have been obtained in the J, H, and K bands using the UCLA Two-Channel IR Camera with a spatial resolution of ~1". The 3'x3' field of view includes over 100 galaxies in each cluster. Photometry has been obtained with 1{sigma} or limiting magnitudes of 21.7 at J, 21.0 at H, and 20.4 at K', and complete to 2 magnitudes fainter than L^*^. Data reduction techniques for flat-fielding object identification, and photometry of faint object crowded fields are discussed. The best method is the subtraction of a running-average sky made from object frames. The photometry is cross referenced to previous catalogs, and infrared color-magnitude diagrams are presented. Comparison of the IR colors of these four clusters to the predictions of the spectral synthesis models of Bruzual and Chariot is discussed. There is a discrepancy between the models and the observations of several tenths of a magnitude in the colors. Photometry has also been obtained for the gravitational lensing arcs in CL 0024+1654, which is consistent with an actively star-forming galaxy at z>1. For a description of the JHK' photometric system, see e.g. <GCPD/09>
Abell 370 ClG 0237.3-0148 02 39.8 -01 35 Abell 963 ClG 1014.2+3917 10 17.2 +39 02 ClG 0024+1654 00 26 32.5 +17 09 43 ClG 0909+4408 09 52 57.1 +43 55 28
JHK' photometry of Abell 370. JHK' Photometry of Abell 963. No Object number in cluster --- BO Butcher and Oemler (1978ApJ...219...18B) number --- xpos x position number=1 1 pix = 0.68". North is up, East is to the left pix ypos y position number=1 1 pix = 0.68". North is up, East is to the left pix n_ypos Note number=2 a : This object is poorly resolved from its neighbor --- Jmag J magnitude (1.2um) mag n_Jmag Note number=2 a : This object is poorly resolved from its neighbor --- Hmag H magnitude (1.65um) mag K'mag K' magnitude (2.1um) mag JHK' photometry of CL 0024+1654 JHK' photometry of CL 0909+4408 No Object number in cluster --- DG Dressler and Gunn (1992, Cat. <J/ApJS/78/1>) number --- xpos x position number=1 1 pix = 0.68". North is up, East is to the left pix ypos y position number=1 1 pix = 0.68". North is up, East is to the left pix n_ypos Note number=2 a : This object is poorly resolved from its neighbor --- Jmag J magnitude (1.2um) mag n_Jmag Note number=2 a : This object is poorly resolved from its neighbor --- Hmag H magnitude (1.65um) mag K'mag K' magnitude (2.1um) mag James Marcout, Patricia Bauer CDS 1997 Sep 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_112_2500.xml Supergiant stars in the disk of NGC 672 J/AJ/112/2559 J/AJ/112/2559 Supergiants in NGC 672 Supergiant stars in the disk of NGC 672 Y -J Sohn T J Davidge Astron. J. 112 2559 1996 1996AJ....112.2559S Photometry, VRI Stars, supergiant V, R, and I CCD images are used to investigate the photometric properties and spatial distribution of supergiants in the nearby interacting galaxy NGC 672. Not counting stars imbedded in H II regions, our sample consists of 237 objects. The (V-R,V-I) two-color diagram indicates that the majority of these stars have spectral types between A-K. Statistical tests show that the outer region of NGC 672 contains a redder population of supergiants than the inner region. Comparisons with theoretical evolutionary tracks indicate that the majority of the supergiants in NGC 672 have progenitor masses between 15M_{sun}_ and 25M_{sun}_, and that the inner regions contain stars that are more massive than in the outer disk, indicating that an age gradient is present. The luminosity functions in all three bandpasses follow power laws, and the exponent in V=0.79+/-0.06, in good agreement with other galaxies. The brightest red supergiants occur at V~22.0, from which we derive a distance modulus of 29.5, corresponding to 7.9(+1.0)(-0.9)Mpc.
NGC 672 01 47 53.2 +27 25 49
Positions, magnitudes, and colors of NGC 672 stars ID Identification number --- Xc X pixel location pix Yc Y pixel location pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag V-I V-I color index mag e_V-I rms uncertainty on V-I mag R-I R-I color index mag e_R-I rms uncertainty on R-I mag HII H II region number from Hodge, 1969ApJ...155..417H --- table2.tex AASTeX version of table2.dat CDS 1997 Jan 31 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 06-Nov-1996 J_AJ_112_2559.xml Carbon Stars in the Large Magellanic Cloud: Luminosities, Colors, and Implications for the History of Star Formation J/AJ/112/2607 J/AJ/112/2607 Carbon Stars in the Large Magellanic Cloud Carbon Stars in the Large Magellanic Cloud: Luminosities, Colors, and Implications for the History of Star Formation E Costa J A Frogel Astron. Jour. 112 2607 1996 1996AJ....112.2607C Magellanic Clouds Stars, carbon Magellanic Clouds stars: carbon stars: formation RI and JHK photometry are presented for 888 and 204 carbon (C) stars, respectively, of the 1035 C stars found by Blanco and his collaborators in 52 fields of the Large Magellanic Cloud (LMC).
The Extinction for each field ID Field --- E_BV Color excess in B-V mag A_I Extinction in I mag E_RI Color excess in R-I mag A_K Extinction in K mag E_JK Color excess in J-K mag E_HK Color excess in H-K mag The observations in R and I ID Star name --- RI_0 Unreddened R-I mag I_0 Unreddened I mag mbol Bolometric magnitude mag JHK Do J, H, and K exist? --- Unreddened magnitudes and JHK photometry ID Star --- I Unreddened I magnitude mag R-I_0 Unreddened R-I color mag K_0 Unreddened K magnitude mag J-K_0 Unreddened J-K coloc mag H-K_0 Unreddened H-K color mag mbol Bolometric magnitude mag Nancy G. Roman ADC/SSDOO 1997 Aug 01 J_AJ_112_2607.xml Faint Cepheid Studies. II. Stars with Published Periods J/AJ/112/2757 J/AJ/112/2757 Faint Cepheid Studies. II Faint Cepheid Studies. II. Stars with Published Periods A A Henden Astron. J. 112 2757 1996 1996AJ....112.2757H J/AJ/111/902 : Short-period Cepheids (Paper I.) (Henden 1996) Photometry, UBVRI Stars, variable UBVRI data on 36 short-period (P<5days) Cepheids is given. The observing techniques and reduction procedures are described. A consistent set of finding charts, a set of standard stars for each Cepheid, and improved coordinates are also presented.
Different instrument systems Code Code --- Obs Observatory --- Tel Telescope --- Filt Filters --- Type Type of photometry number=1 PEP: Early photoelectric photometry, before 1987 CCD: CC photometry starting in 1985 --- Dec Detector --- Ap Aperture arcsec Comparison stars Name Variable star name --- Comp Comparison star number --- GSC Guide Star Catalog number (if available) --- RAh Right Ascension (J2000) h --- Always ':' --- RAm Right Ascension (J2000) min --- Always ':' --- RAs Right Ascension (J2000) s DE- Sign, Declination --- DEd Declination (J2000) deg --- Always ':' --- DEm Declination (J2000) arcmin --- Always ':' --- DEs Declination (J2000) arcsec Vmag V magnitude mag e_Vmag Error in Vmag mag B-V B-V color mag e_B-V Error in B-V mag U-B U-B color mag e_U-B Error in U-B mag V-R V-R color mag e_V-R Error in V-R mag R-I R-I color mag e_R-I Error in R-I mag Photometric data Name Variable star name --- HJD Heliocentric Julian date JD Vmag V magnitude mag e_Vmag Error in Vmag 10-3mag B-V B-V color mag e_B-V Error in B-V 10-3mag U-B U-B color mag e_U-B Error in U-B 10-3mag V-R V-R color mag e_V-R Error in V-R 10-3mag R-I R-I color mag e_R-I Error in R-I 10-3mag Code Instrument system code from table 1 --- table3.tex AASTeX version of table3.dat table4.tex AASTeX version of table4.dat CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 30-Mar-1997 J_AJ_112_2757.xml The Behlen Observatory variable star survey: Paper IV J/AJ/112/2769 J/AJ/112/2769 Behlen Observatory Survey. IV. The Behlen Observatory variable star survey: Paper IV E G Schmidt A Seth Astron. J. 112 2769 1996 1996AJ....112.2769S J/AJ/106/2429 : Behlen Obs. variables stars survey (Schmidt+, 1993) Photometry Stars, variable Finding charts, accurate coordinates, and light curves are presented for 106 variable stars including 6 which are newly discovered. Parameters descriptive of the light curves are tabulated including periods for 16 stars which lacked them. The periods from the General Catalog of Variable Stars for ten stars were found to be seriously in error. The classification of the stars is discussed. Revisions or refinements of the classifications from the General Catalogue of Variable Stars are suggested for 20 stars and classifications are given for 7 which were previously unclassified. 15%-23% of the Bailey type ab RR Lyrae stars show scatter in their light curves which is suggestive of the Blazhko effect.
Photometric data Name Star name --- HJD Heliocentric Julian Date d Phase Phase --- Vmag V magnitude mag Rmag R magnitude mag V-R V-R color mag Flag Flag indicating uncertainty --- Identification and coordinates of variables Name Star name --- Type Variable type --- n_Type Note for V652 Her number=1 V652 Her: unique variable, see the GCVS (Cat. <II/139>) --- GSC GSC (Cat. <II/143>) number --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec James Marcout, Patricia Bauer CDS 1997 Jan 31 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 06-Nov-1996 UNKNOWN UNKNOWN Table2 prepared via OCR at CDS, corrected on 16-Apr-1997 J_AJ_112_2769.xml The TIRGO lunar occultation program: summary of the 1985-1995 observations. J/AJ/112/2786 J/AJ/112/2786 1985-1995 lunar occultations at TIRGO The TIRGO lunar occultation program: summary of the 1985-1995 observations. A Richichi C Baffa G Calamai F Lisi Astron. J. 112 2786 1996 1996AJ....112.2786R Occultations Photometry, infrared astrometry binaries: close binaries: general binaries: visual occultations A program of observations of lunar occultations in the near-infrared was started at the TIRGO observatory in late 1985. After ten years of operation, we provide a list of all the events recorded up to the end of 1995 using the facility IR photometer. A total of 157 light curves were obtained, mostly aiming at measurements of angular diameters and binaries, with a total of 54 results in these fields. In Table 1 is reported a summary of the occultation events and the parameters of their observations. In Table 2 is reported a list of cross-identifications, coordinates, and characteristics.
Occultation Parameters N. Event sequential identification number --- Name Source name --- Date UT date of event --- Dark Night- or day-time flag N = night-time D = day-time --- Event Circumstance of event R = reappearance D = disappearance --- Filter Filter used J,H,K,L = broadband filter name # = narrow band around 2.16um For details see AJ,112,2786. --- Diaphr Diaphragm used Diaphragm diameter (equivalent seconds of arc on the sky). arcsec IntTime Integration time in ms ms SampTime Sampling time in ms ms Gain Charge preamplifier gain used Charge preamplifier gain. L = low gain H = high gain --- CA Contact angle Contact angle, that is the predicted angle between the direction of the lunar motion and the contact angle (degrees). deg PA Position angle Position angle, that is the predicted angle along which the Moon's limb scanned the source (degrees). deg SNR Signal to noise ratio Signal to noise ratio as measured on the ligthcurve. --- Rem. Remarks D = resolved angular diameter S = circumstellar shell B = binary 50Hz = data affected by strong 50Hz pick-up Sat. = part of the lightcurve was saturated 2b = gap between the blocks eob = data near the edge of a block --- Ref. References 1 = Richichi, A. 1987, Mem. Soc. Astron. Ital., 58, 431 (1987MmSAI..58..431R) 2 = Richichi, A., Salinari, P., Lisi, F. 1988, Astrophys. J., 326, 791 (1988ApJ...326..791R) 3 = Richichi, A. 1989, Astron. Astrophys., 226, 366 (1989A&A...226..366R) 4 = Richichi, A., Di Giacomo, A., Lisi, F., Calamai, G., 1992, Astron. Astrophys., 265, 535 (1992A&A...265..535R) 5 = Richichi, A., Calamai, G., Leinert, Ch., Stecklum, B., Trunkovsky, E.M. 1996a, Astron. Astrophys., 309, 163 (1996A&A...309..163R) 6 = Richichi, A., Lisi, F., Calamai, G. 1991, Astron. Astrophys., 241, 131 (1991A&A...241..131R) 7 = Richichi, A., Calamai, G., Leinert, Ch. 1994, Astron. Astrophys., 286, 829 (1994A&A...286..829R) 8 = Di Giacomo, A., Richichi, A., Lisi, F., Calamai, G. 1991, Astron. Astrophys., 249, 397 (1991A&A...249..397D) 9 = Richichi, A., et al. 1995,A&A, 301, 439 (1995A&A...301..439R) 10 = Richichi, A., Calamai, G., Leinert, Ch., Stecklum, B., 1996b, Astron. Astrophys., accepted (1997A&A...322..202R) --- X-id, V,K and Sp N. Identification number of Table 1 --- SAO Source SAO number --- HD Source HD number --- IRC Source IRC number --- Other Other source name --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec Vmag V magnitude mag u_Vmag Note on V magnitude --- Kmag K magnitude mag u_Kmag Note on K magnitude a = K magnitude derived from the V magnitude and the color for the assumed spectral type. b = K magnitude derived from the intensity of the signal during the occultation event. --- Sp Spectral type --- UNKNOWN 1997 May 07 J_AJ_112_2786.xml UBV Photometry of Southern Luminous Stars J/AJ/112/2855 J/AJ/112/2855 UBV Photometry of LSS stars UBV Photometry of Southern Luminous Stars C B Reed S J Vance Astron. J. 112 2855 1996 1996AJ....112.2855R III/43 : Luminous Stars in the Southern Milky Way (Stephenson+ 1971) J/AJ/106/2291 : UBV photometry toward Galactic Center (Reed 1993) J/PASP/105/1465 : Distant OB Stars in the Galaxy (Reed 1993) J/ApJS/87/367 : UBV-beta database for LS stars (Reed, 1993) J/ApJS/97/189 : Spectroscopic Database for LSS (Reed+ 1995) J/A+AS/117/313 : Stroemgren photometry of LSS stars (Reed, 1996) J/AJ/113/823 : Radial velocity database for LSS stars (Reed+ 1997) Photometry, UBV Stars, luminous UBV photometry of 284 stars listed in Stephenson and Sanduleak's Luminous Stars in the Southern Milky Way catalog (Cat. <III/43>) is reported. (Copyright) 1996 American Astronomical Society.
LS Star photometry LS Luminous Stars (Sanduleak, Cat. <III/43>) number --- Vmag V magnitude mag B-V B-V color mag U-B U-B color mag Nobs Number of times star was observed --- e_Vmag Std. dev. in Vmag mag e_B-V Std. dev. in B-V mag e_U-B Std. dev. in U-B mag HD/CD HD or CD cross-identification --- Sp Spectral type and notes The spectral type of the star, plus any notes. If an asterisk, "*", appears in the last column, an additional note for the star appears below: 2541 LS catalog notes possible composite spectrum 2801 Companion to northeast, outside diaphragm, {delta}m~2-3mag. 2831 Close faint companion immediately to south, {delta}m~3mag. 3074 LS catalog notes possible {lambda}4686 emission 3261 Companion to northeast just inside diaphragm; {delta}m~3mag. 3501 LS catalog notes H{beta} weak 3541 LS catalog notes He enhanced 4234 Identification uncertain 4601 Faint companion immediately to southwest; inside diaphragm 4793 Double; companion to south, {delta}m~1mag. 4909 LS catalog notes possible {lambda} 4650-86 emission 5041 Companion immediately to east; inside diaphragm. {delta}m~2mag. 5060 Crowded by bright star 5104 LS catalog notes H{beta} weak --- CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 30-Mar-1997 J_AJ_112_2855.xml The MSX Infrared Astrometric Catalog, Version 4.2.1 J/AJ/112/2862 J/AJ/112/2862 The MSX Infrared Astrometric Catalog The MSX Infrared Astrometric Catalog, Version 4.2.1 M P Egan Astron. J. 112 2862 1996 1996AJ....112.2862E I/149A : FK5 (Fricke+1988) I/175 : FK5 Extension (Fricke+1991) I/171 : ACRS (Corbin+ 1991) I/146 : PPM (Roeser+ 1988) I/193 : PPM South (Bastian+ 1991) II/184 : CIO (Gezari+ 1993) http://www.plh.af.mil/gpo/ : The MSX IR Astrometric Catalog, Version 4.2.1 Astrometric data Infrared sources The MSX IR Astrometric Catalog, Version 4.2.1 was constructed to provide improved pointing accuracy of infrared observations. The catalog contains 177,860 stars, 61,242 which are in either an IRAS catalog and/or the Catalog of Infrared Observations. The catalog was constructed from a number of visible astrometric catalogs, and contains position information accurate to the sub-arcsecond level. The FK5 (1988 Fricke Schwan and Lederle), FK5 Extension (1991 Fricke, Schwan and Corbin), Astrographic Catalog of Reference Stars (1991 Corbin and Urban), Position and Proper Motion Catalog (1988 Roeser and Bastian) and PPM South (1991 Bastian et al.) were the sources of position and magnitude information. The PPM and FK5 catalogs contain 1-D spectral type information, and this was supplemented where possible with 2-D MK spectral types. The ACRS and PPM quote photographic magnitudes. These were transformed to V magnitude using the spectral type and expected B-V color. The catalog lists astrometric source catalog identification, IR name, equatorial position at J2000 and proper motions with errors, spectral type, IRAS or CIO flux in 12, 25, 60, 100 micron bands, and estimates of flux in the MSX SPIRIT III instrument IR bands.
MSX
Main Catalog, Flux units (Jy) ASTROM_ID Original astrometric catalog ID The catalog ID's referred to are: Astrometric Catalog ASTROM_ID ___________________________________________ FK5 F FK5 Extension f ACRS A PPM N PPM South S Infrared Catalog IR_ID ___________________________________________ IRAS Point Source Catalog P IRAS Faint Source Catalog F Combined PSC/FSC data B IRAS Faint Source Reject Z IRAS Serendipitous Survey S Catalog of IR Observations C ___________________________________________ --- ASTROM_NUM astrometric catalog number --- IR_ID IR catalog ID --- ID_name Name of star in IR catalog --- RAh R.A. hours (J2000) h RAm R.A. minutes (J2000) min RAs R.A. seconds (J2000) s DE- sign of declination --- DEd declination degrees (J2000) deg DEm declination arcminutes (J2000) arcmin DEs declination arcseconds (J2000) arcsec e_RA mean R.A. error*cos(dec), 0.001 sec of time ms e_DE mean declination error, 0.01 seconds of arc 10marcsec PMRA proper motion in R.A., (J2000) in s of time/Julian cy c.s/yr PMDE proper motion in dec., (J2000) in sec of arc/Julian cy c.arcsec/yr e_PMRA mean error of R.A. PM*cos(dec) in 0.001s of time/cy 10us/yr e_PMDE mean error of dec PM, 0.01 s of arc/cy 0.1marcsec/yr Sp spectral type --- Lc luminosity class (e.g. 3 = III; 0 = none) --- IRAS_LRS_ID IRAS LRS designation --- Vmag visual magnitude, V mag F(12) IRAS 12 micron flux or wavelength of CIO obs. Jy F(25) IRAS 25 micron flux or flux of CIO obs. Jy F(60) IRAS 60 micron flux or wavelength of CIO obs. Jy F(100) IRAS 100 micron flux or flux of CIO obs. Jy q_F(12) IRAS 12 micron flux quality flag, fqual(1); --- q_F(25) IRAS 25 micron flux quality flag, fqual(2); --- q_F(60) IRAS 60 micron flux quality flag, fqual(3); --- q_F(100) IRAS 100 micron flux quality flag, fqual(4); --- SP3(A) SPIRIT III Band A flux density estimate Jy SP3(B1) SPIRIT III Band B1 flux density estimate Jy SP3(B2) SPIRIT III Band B2 flux density estimate Jy SP3(C) SPIRIT III Band C flux density estimate Jy SP3(D) SPIRIT III Band D flux density estimate Jy SP3(E) SPIRIT III Band E flux density estimate Jy est_F(12) 12 micron flux density estimate Jy Main Catalog, Irradiance units ASTROM_ID Original astrometric catalog ID The catalog ID's referred to are: Astrometric Catalog ASTROM_ID ___________________________________________ FK5 F FK5 Extension f ACRS A PPM N PPM South S Infrared Catalog IR_ID ___________________________________________ IRAS Point Source Catalog P IRAS Faint Source Catalog F Combined PSC/FSC data B IRAS Faint Source Reject Z IRAS Serendipitous Survey S Catalog of IR Observations C ___________________________________________ The Appendix to version 4.2 contains 1538 bright IR stars with good positions (2 - 3 arcsecond accuracy) determined from the Two-micron Sky Survey. app_j.dat and app_i.dat are ASCII files, written in identical formats to the main catalog. A number of the fields have taken on different meanings. As above, only the units of the SPIRIT III band flux estimates differ between the files. The following tables list the format of each file. --- ASTROM_NUM astrometric catalog number --- IR_ID IR catalog ID --- ID_name Name of star in IR catalog --- RAh R.A. hours (J2000) h RAm R.A. minutes (J2000) min RAs R.A. seconds (J2000) s DE- sign of declination --- DEd declination degrees (J2000) deg DEm declination arcminutes (J2000) arcmin DEs declination arcseconds (J2000) arcsec e_RA mean R.A. error*cos(dec), 0.001 sec of time ms e_DE mean declination error, 0.01 seconds of arc 10marcsec PMRA proper motion in R.A., (J2000) in s of time/Julian cy cs/a PMDE proper motion in dec., (J2000) in sec of arc/Julian cy carcsec/a e_PMRA mean error of R.A. PM*cos(dec) in 0.001s of time/cy 10us/a e_PMDE mean error of dec PM, 0.01 s of arc/cy 0.1marcsec/a Sp spectral type --- Lc luminosity class (e.g. 3 = III; 0 = none) --- IRAS_LRS_ID IRAS LRS designation --- Vmag visual magnitude, V mag F(12) IRAS 12 micron flux or wavelength of CIO observation Jy F(25) IRAS 25 micron flux or flux of CIO obs. Jy F(60) IRAS 60 micron flux or wavelength of CIO obs. Jy F(100) IRAS 100 micron flux or flux of CIO obs. Jy q_F(12) IRAS 12 micron flux quality flag, fqual(1); --- q_F(25) IRAS 25 micron flux quality flag, fqual(2); --- q_F(60) IRAS 60 micron flux quality flag, fqual(3); --- q_F(100) IRAS 100 micron flux quality flag, fqual(4); --- SP3(A)i SPIRIT III Band A in-band irradiance est. W/cm2 SP3(B1)i SPIRIT III Band B1 in-band irradiance est. W/cm2 SP3(B2)i SPIRIT III Band B2 in-band irradiance est. W/cm2 SP3(C)i SPIRIT III Band C in-band irradiance est. W/cm2 SP3(D)i SPIRIT III Band D in-band irradiance est. W/cm2 SP3(E)i SPIRIT III Band E in-band irradiance est. W/cm2 est_F(12) 12 micron flux density estimate Jy Appendix, FLux units (Jy) ASTROM_ID (IRC) Original astrometric catalog ID --- ASTROM_NUM name in IRC catalog --- IR_ID (PSC) IR catalog ID --- ID_name Name of star in IRAS PSC --- RAh R.A. hours (J2000) h RAm R.A. minutes (J2000) min RAs R.A. seconds (J2000) s DE- sign of declination --- DEd declination degrees (J2000) deg DEm declination arcminutes (J2000) arcmin DEs declination arcseconds (J2000) arcsec e_RA mean R.A. error*cos(dec), 0.001 sec of time ms e_DE mean declination error, 0.01 seconds of arc 10marcsec NULL-1 NULL-1 --- NULL-2 NULL-2 --- NULL-3 NULL-3 --- NULL-4 NULL-4 --- Sp spectral type - blank --- Lc Luminosity class - blank --- IRAS_LRS_ID IRAS LRS designation --- Kmag K magnitude (2.2 microns) mag F(12) IRAS 12 micron flux or wavel. of CIO obs. Jy F(25) IRAS 25 micron flux or flux of CIO obs. Jy F(60) IRAS 60 micron flux or wavel. of CIO obs. Jy F(100) IRAS 100 micron flux or flux of CIO obs. Jy q_F(12) IRAS 12 micron flux quality flag, fqual(1); --- q_F(25) IRAS 25 micron flux quality flag, fqual(2); --- q_F(60) IRAS 60 micron flux quality flag, fqual(3); --- q_F(100) IRAS 100 micron flux quality flag, fqual(4); --- SP3(A) SPIRIT III Band A flux density estimate Jy SP3(B1) SPIRIT III Band B1 flux density estimate Jy SP3(B2) SPIRIT III Band B2 flux density estimate Jy SP3(C) SPIRIT III Band C flux density estimate Jy SP3(D) SPIRIT III Band D flux density estimate Jy SP3(E) SPIRIT III Band E flux density estimate Jy est_F(12) 12 micron flux density estimate Jy Appendix, Irradiance Units ASTROM_ID (IRC) Original astrometric catalog ID --- ASTROM_NUM name in IRC catalog --- IR_ID (PSC) IR catalog ID --- ID_name Name of star in IRAS PSC --- RAh R.A. hours (J2000) h RAm R.A. minutes (J2000) min RAs R.A. seconds (J2000) s DE- sign of declination --- DEd declination degrees (J2000) d DEm declination arcminutes (J2000) arcmin DEs declination arcseconds (J2000) arcsec e_RA mean R.A. error*cos(dec), 0.001 sec of time ms e_DE mean declination error, 0.01 seconds of arc 10marcsec NULL-1 NULL-1 --- NULL-2 NULL-2 --- NULL-3 NULL-3 --- NULL-4 NULL-4 --- Sp spectral type - blank --- Lc Luminosity class - blank --- IRAS_LRS_ID IRAS LRS designation --- Kmag K magnitude (2.2 microns) mag F(12) IRAS 12 micron flux or wavel. of CIO obs. Jy F(25) IRAS 25 micron flux or flux of CIO obs. Jy F(60) IRAS 60 micron flux or wavel. of CIO obs. Jy F(100) IRAS 100 micron flux or flux of CIO obs. Jy q_F(12) IRAS 12 micron flux quality flag, fqual(1); --- q_F(25) IRAS 25 micron flux quality flag, fqual(2); --- q_F(60) IRAS 60 micron flux quality flag, fqual(3); --- q_F(100) IRAS 100 micron flux quality flag, fqual(4); --- SP3(A) SPIRIT III Band A flux density estimate W/cm2 SP3(B1) SPIRIT III Band B1 flux density estimate W/cm2 SP3(B2) SPIRIT III Band B2 flux density estimate W/cm2 SP3(C) SPIRIT III Band C flux density estimate W/cm2 SP3(D) SPIRIT III Band D flux density estimate W/cm2 SP3(E) SPIRIT III Band E flux density estimate W/cm2 est_F(12) 12 micron flux density estimate Jy doc.ps Full postscript documentation doc.txt Abbreviated ascii documentation fig_1_2.ps Figure 1 and 2 fig_3_4.ps Figure 3 and 4 fig_5.ps Figure 5 fig_6.ps Figure 6 fig_7_8.ps Figure 7 and 8 fig_9.ps Figure 9 fig_10.ps Figure 10 N Paul Kuin NASA/ADC 1997 Apr 29 UNKNOWN UNKNOWN The catalog was prepared to provide pointing to the SPIRIT III infrared telescope on board the Midcourse Space Experiment Mission (MSX) of the Ballistic Missile Organization (BDMO) which has a 30 times better spatial resolution than the IRAS mission. Spatial coincidence and color-matching criteria (based on V-[12] color and spectral type) were used to identify IR counterparts of the astrometric stars. The IRAS Point Source, Faint Source, Faint Source Reject file, and Serendipitous Survey catalogs were used to supply IR observations, as was the Catalog of Infrared Observations (1993 Gezari et al.). The IR flux in each SPIRIT III band was estimated using the V magnitude, spectral type, and IR flux (if available) to determine a blackbody spectrum for the star, which was then convolved with the system spectral response of each SPIRIT III radiometer band. Stars which were brighter than 8th magnitude in band A were retained in the final MSX IR astrometric catalog. The original version of the catalog, MSX4_2_1 quotes SPIRIT III source flux density (Jansky's) at the effective wavelength of each band. In the secondary version of the catalog, MSX4_2_1A, the in-band irradiance of each source in each band is quoted, in units of Watts per square centimeter. Both cat_j.dat and cat_i.dat are ASCII files, written in identical formats. Only the units of the SPIRIT III band flux estimates are different, as noted above. The following tables list the format of each catalog file. J_AJ_112_2862.xml A morphological catalog of galaxies in the Hubble Deep Field J/AJ/112/359 J/AJ/112/359 Galaxies in the Hubble Deep Field A morphological catalog of galaxies in the Hubble Deep Field S van den Bergh R G Abraham R S Ellis N R Tanvir B X Santiago K G Glazebrook Astron. J. 112 359 1996 1996AJ....112..359V Galaxies, photometry Morphology We present a catalog of morphological and color data for galaxies with 21<I_814<25mag in the Hubble Deep Field (Williams et al. 1996, in Science with the Hubble Space Telescope II). Galaxies have been inspected and (when possible) independently visually classified on the MDS and DDO systems. Measurements of central concentration and asymmetry are also included in the catalog. The fraction of interacting and merging objects is seen to be significantly higher in the Hubble Deep Field than it is among nearby galaxies. Barred spirals are essentially absent from the deep sample. The fraction of early-type galaxies in the Hubble Deep Field is similar to the fraction of early-types in the Shapley-Ames Catalog, but the fraction of galaxies resembling archetypal grand-design late-type spiral galaxies is dramatically lower in the distant HDF sample.
Catalog of HDF classifications ID Galaxy ID number --- n_ID Notes presence of Lyman discontinuity The 42 high-z candidates with red UV-optical colors (U_300-B_450>-0.2) and blue optical-near IR colors (V_606-I_814>-0.6), indicating the possible presence of the Lyman discontinuity in the U_300-band spectral energy distribution (Steidel et al., 1996ApJ...462L..17S), are indicated by an asterisk in this column. --- RAh Right ascension, J2000 h RAm Right ascension, J2000 min RAs Right ascension, J2000 s DE- Declination sign --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec Xpos X pixel coord. on v.2 "drizzled" image Pixel coordinates on the version 2 "drizzled" HDF frames released by STScI. The first digit in the ID numbers corresponds to the WF/PC2 chip on which the object lies. Note also that positions were originally measured on the version 1 drizzled images, and were converted to version 2 coordinates using (x,y)_v1=76+(x,y)+v2 (M. Dickinson, private communication). pix Ypos Y pixel coord. on v.2 "drizzled" image pix Imag I_814 magnitude mag U-B U_300-B_450 color index mag B-V B_450-V_606 color index mag V-I V_606-I_814 color index mag Asym Asymmetry --- Conc Central concentration measure Color concentration measure from Abraham et al., (1996MNRAS.279L..47A). --- RSE Visual classification by RSE Visual classification by RSE into three large bins (E = elliptical, S=spiral, P=irregular/peculiar/merger). --- vdB Visual classification by vdB Visual classification by vdB on the numerical "MDS system" used by RSE to classify the data in Glazebrook et al, (1995MNRAS.275L..19G) and described in detail in Abraham et al. (1996ApJS..107....1A). --- Desc Galaxy class. by vbD on DDO system Galaxy classification by vdB on the DDO system. All uncertain classifications are followed by a colon. --- Note Notes on classification Notes on the DDO classifications and remarks on the colors of individual galaxies are given: notes on classifications: a: possibly a very distant Sc viewed in UV b: asymmetrical c: companion to 2-220 d: has faint companions e: companion to 2-299 f: good example of merger g: has companions h: has companion i: has bright companions j: companion to 3-267 k: has bright bar-like core l: has bright companion m: part of spiral (?) arm of 3-296 n: companion to 3-426 o: star off center p: companion to 3-426 q: companion to 3-517 r: chain galaxy? s: interacting with 3-606 t: companion to 4-105 u: companion to 4-387 v: gravitational lens? w: companion to 4-655 x: red nucleus y: blue outer knots z: Ir? companion vR aa: "tadpole" with R head and B tail ab: Pec component vB ac: blue compact companion ad: has one blue arm ae: one component R af: triple merger, all components B ag: or tadpole galaxy af: E1 galaxy is R, companion is B notes on colors of individual galaxies: vB: very blue B: blue R: red vR: very red --- table1.tex Modified AASTeX version of table1.dat CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 03-Oct-1996 J_AJ_112_359.xml Dynamics of the cluster of galaxies A3266 (SERSIC 40/6). I. Spectroscopic data J/AJ/112/36 J/AJ/112/36 Velocities in Abell 3266 Dynamics of the cluster of galaxies A3266 (SERSIC 40/6). I. Spectroscopic data H Quintana A Ramirez M J Way Astron. J. 112 36 1996 1996AJ....112...36Q Clusters, galaxy Galaxies, spectra Radial velocities We present 387 velocities covering an area 1.8x1.8deg^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.
A3266 - Velocities. Id Identification number --- RAh Right ascension (1950) h mAh Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vel Velocity km/s e_Vel rms uncertainty on Vel km/s R R Tonry and Davis (1979AJ.....84.1511T) value Mpc Note emission/uncertainty number=1 e: presence of emission lines *: Velocities noted as uncertain by TCG90 that presents a great disagreement with our data --- Ref References number=2 This paper: argu = ARGUS spectra fibr = LCO fiber spectra shec = re-measured by Quintana and Ramirez (1990AJ....100.1121Q) Others: C085 = Carter et al. (1985MNRAS.212..471C) G088 = Green et al. (1988MNRAS.234.1051G) M082 = Materne et al. (1982A&A...109..238M) MQ81a = Melnick and Quintana (1981A&AS...44...87M) MQ81b = Melnick and Quintana (1981AJ.....86.1567M) TCG90 = Teague et al. (1990ApJS...72..715T) V075 = Vidal (1975PASP...87..625V) W080 = West and Frandsen (1981A&AS...44..329W) --- IdRef Fiber or galaxy number in the references number=3 A negative value indicates that the velocity was not used in the calculation --- VelAdop Adopted final velocity km/s e_VelAdop rms uncertainty on VelAdop km/s James Marcout, Patricia Bauer CDS 1997 Apr 10 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_112_36.xml Late-Type Stars in M31. II. C-, S-, and M-Star Spectra J/AJ/112/491 J/AJ/112/491 Late-Type Stars in M31. II. Late-Type Stars in M31. II. C-, S-, and M-Star Spectra J P Brewer H B Richer D R Crabtree Astron. J. 112 491 1996 1996AJ....112..491B J/AJ/109/2480 : Late-type stars in M31. I. (Brewer+ 1995) Spectroscopy Stars, late-type The files with the prefix CFHT contain the M31 spectra, the files files with the prefix DAO contain spectra of Galactic carbon stars. See the text of the printed paper for details. Only encapsulated PostScript version of the spectra are available. We present spectra of AGB stars in M31 for which observations had been previously secured using a four-band photometric system (FBPS). The FBPS had been used to identify M-, S-, and carbon-star (C-star) candidates, and we use the spectra to show that the FBPS did an excellent job at identifying C- and M-stars. Of the 48 C-stars for which spectra were obtained, 7 have strongly enhanced 13C bands (J-stars), 2 have strong Halpha emission, while 3 are found to exhibit enhanced Li absorption (Li-stars). Both the J- and Li-stars are fainter than predicted by current theoretical models, while the colors of the Halpha stars suggest they may be in the terminal phases of their evolution. The C2 and CN band strengths of the C-stars are measured, and no correlation between these band strengths and either Mbol or (V-I) is found. It is suggested that this lack of correlation is due to an age spread. The spectra of the first confirmed S-star in M31 is presented, and two evolutionary pathways are suggested to account for this star's high luminosity.
CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 10-Aug-1996 J_AJ_112_491.xml Proton capture chains in globular cluster stars. I. Evidence for deep mixing based on sodium and magnesium abundances in M13 giants J/AJ/112/545 J/AJ/112/545 Proton capture chains in globular clusters. I. Proton capture chains in globular cluster stars. I. Evidence for deep mixing based on sodium and magnesium abundances in M13 giants C A Pilachowski C Sneden R P Kraft G E Langer Astron. J. 112 545 1996 1996AJ....112..545P Abundances Clusters, globular Effective temperatures Stars, giant Sodium abundances have been derived for 130 giant stars in the globular cluster M13 from spectra of the Na I doublet at {lambda}5682 and 5685A obtained using the KPNO 4-m Hydra fiber positioner and bench spectrograph. Magnesium abundances have also been obtained for the brightest 98 stars in the sample from the nearby Mg I line at {lambda}5711A. The stars observed in M13 range from the faintest at M_V_~+1.0 and log(g)~2.6 up to the tip of the giant branch, and include 18 stars on the asymptotic giant branch. Among the lower luminosity giants, the sodium abundances have a large star-to-star range, approximately from -0.3<=[Na/Fe]<=+0.5. However, the sodium abundances of the most luminous giants (Mv<-1.7) are usually high; typically, [Na/Fe]>=+0.3, with a much smaller star-to-star scatter. The asymptotic giant branch stars have smaller sodium abundances on average than do the red giant branch tip stars. The spread in [Na/Fe] ratios is larger in M13 than it is among halo field giants of comparable metallicity; M13 contains many more stars with high [Na/Fe] ratios than can be found in the field, even at relatively low luminosities on the giant branch. Magnesium is uniformly overabundant ([Mg/Fe]~+0.3) in all stars with a low sodium abundance, but the [Mg/Fe] ratio ranges from approximately -0.3 to +0.3 in stars with a high sodium abundance. These sodium and magnesium abundance variations in M13 are discussed in the context of proton capture and deep mixing hypotheses. In addition to the CN and ON hydrogen burning chains previously discussed in the literature, the NeNa and MgAl burning chains have also contributed to the abundance mixture observed in M13 giants. At least some of the products of proton capture chains have been produced in situ in the giants, and brought to the surface, most probably via deep mixing. Evidence in support of the occurrence of proton capture nucleosynthesis and deep mixing among M13 stars includes (1) the absence of sodium-poor stars at the red giant tip, (2) the fact that asymptotic branch stars have lower sodium abundances on average than do stars near the red giant tip, and (3) the existence of a positive correlation between sodium and nitrogen abundances as well as a partial anti-correlation of sodium and magnesium abundances.
M 13 NGC 6205 16 41.7 +36 27
M13 star basic data and results Star Primary designation Primary star name references: L = Ludendorf, (1905POPot..50....1L) K = Kadla, (1966IzPul.181...93K) CM = Cudworth & Monet, (1979AJ.....84..774C) --- Alt Alternate designation Alternate star name references: SA, SB = Savedoff, (1956AJ.....61..254S) V (variable stars) = Hogg, (1973PDDO....3....6S) BAUM = Baum, (1954AJ.....59..422B) "Roman numerals" = Arp, (1955AJ.....60..317A) remaining designations appear either in Arp & Johnson, (1955ApJ...122..171A) (their Figure 4) or in Sandage, (1970ApJ...162..841S) (his Figure 5). --- Vmag V magnitude V and B-V from Cudworth & Monet, (1979AJ.....84..774C) mag B-V B-V color mag Mvo Estimated absolute V magnitude mag Branch Evolutionary status (Red Giant Branch, RGB, Asymptotic Giant Branch, AGB) --- u_Branch Branch uncertainty flag --- Code Analysis code Definitions of the code numbers: 1 = good enough spectrum to derive both sodium and magnesium abundances 2 = good enough spectrum to derive a sodium abundance, but not magnesium 3 = essentially no flux in the reduced spectrum; mis-positioned fiber? 4 = very weak absorption spectrum; possibly a warm star? 5 = hot horizontal branch star 6 = poor signal-to-noise in the reduced spectrum --- Teff Effective temperature K log(g) log(10) of the surface gravity cm/s2 vt Microturbulence km/s [Na/Fe] Sodium abundance relative to iron --- [Mg/Fe] Magnesium abundance relative to iron --- table1.tex AASTeX version of table1.dat UNKNOWN 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 13-Aug-1996 J_AJ_112_545.xml UIT: New ultraviolet stellar photometry and surface brightness profiles of the globular cluster M 79 (NGC 1904) J/AJ/112/601 J/AJ/112/601 UV photometry in M79 UIT: New ultraviolet stellar photometry and surface brightness profiles of the globular cluster M 79 (NGC 1904) R S Hill K -P Cheng E P Smith P M N Hintzen R C Bohlin R W OConnell M S Roberts A M Smith T P Stecher Astron. J. 112 601 1996 1996AJ....112..601H Clusters, globular Photometry, ultraviolet Ultraviolet photometry is presented for the globular cluster M79 (NGC 1904) according to the final calibration of the images obtained on the Astro-1 Spacelab mission by the Ultraviolet Imaging Telescope. These results include both point-source and surface photometry at 152nm and 249nm. An ultraviolet color-magnitude (C-M) diagram in these bandpasses is presented. The detected stars are also cross-matched with the ground-based photometry of Ferraro et al. (1992MNRAS.256..391F) to produce C-M and two-color diagrams covering a 4000A span in wavelength. The observed horizontal branch (HB) is compared with stellar interior models of the zero-age HB (ZAHB). Many stars are found in post-HB evolutionary stages more luminous than the ZAHB. The distribution of stars along the ZAHB in m152-m249 color is investigated, and an indication of possible bimodality is found. The relative population of the blue HB tail may vary with radius for radii greater than 1'. Ultraviolet surface brightness and color-index profiles are presented. The previously reported central gradient in the m152-V color index is confirmed, and a faint diffuse component is detected outside a radius of 40" in the 152nm band. Two possible causes of the central color gradient are discussed: mass segregation, and the destruction of red giant envelopes by enhanced mass loss in the cluster core.
ASTRO 1/UIT
UV stellar photometry of M79 Star Ordinal number of UIT-detected star in M79 --- Note Table note mark Table note mark "g": Star 94=UIT-1 and star 76 = UIT-2 as discussed in Paper I (Hill, R. S. et al. 1992ApJ...395L..17H). Stars 26, 67, 100, 109, and 127 are in the area observed by F92 but have no F92-HB match with B-V<0.4. Stars 111, 120, and 122 are ambiguously matched by two or more F92 (1992MNRAS.256..391F) HB stars. --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec m152 UIT magnitude in the 152nm (B1) band UIT magnitude in the 152nm (B1) band. Magnitudes are defined as -2.5*log(flux)-21.1, where log is base 10, and flux is f sub lambda in units of ergs/cm2/s/A. mag C152-249 UIT color index 152nm (B1) - 249nm (A1) mag e_m152 Formal error in UIT 152nm (B1) magnitude mag e_m249 Formal error in UIT 249nm (A1) magnitude mag R Distance of UIT source from cluster center arcsec Qnote Note on quality of observation Note on quality of observation. *: UIT source is within 5 pixels (5.7arcsec) of more than one HB star of F92; if an F92 number is given, it is judged the most likely candidate according to color index and distance from the UIT source position. C: Obvious crowding in one or both UIT bands, as determined by inspection; stars without this note may still be affected by crowding if r<~40arcsec. Lowercase f or n: An aperture magnitude is substituted for a PSF magnitude with error greater than 0.2mag, for image FUV0141 or NUV0124, respectively. Entries 134-136 have aperture photometry only. --- IDF92 Star number from Ferraro et al., 1992 The complete reference F92 is the following: Ferraro, F. R., Clementini, G., Fusi Pecci, F., Sortino, R., and Buonanno, R., (1992MNRAS.256..391F) --- B-VF92 B-V color index from Ferraro et al., 1992 mag VmagF92 V magnitude from Ferraro et al., 1992 mag CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 13-Aug-1996 J_AJ_112_601.xml A study of quasar absorption-line systems with IRAS J/AJ/112/62 J/AJ/112/62 Quasar absorption-line systems A study of quasar absorption-line systems with IRAS A M Tanner J Bechtold C E Walker J H Black R M Cutri Astron. J. 112 62 1996 1996AJ....112...62T Photometry, infrared QSOs Redshifts A survey of quasar absorbers was conducted using the Infrared Astronomical Satellite (IRAS) database. Quasars with known intervening absorption-line systems and broad absorption line (BAL) QSOs were selected primarily from Junkkarinen et al. (1991ApJS...77..203J). Of the 570 quasars with IRAS data, 52 showed 3{sigma} or better detections in at least one band in SCANPI analysis. The origin of the IRAS flux could be from the absorption-line systems, other galaxies, or the quasar itself. The spectral energy distributions for quasars detected in the absorption-line sample and BAL QSOs were found to be redder than those of two control samples which suggests that some of the IRAS flux may arise in dust associated with the intervening galaxies. IRAS SUPERSCANPI processing was carried out for 77 quasars with known Mg II absorption at Zabs<1 to investigate the ensemble far-infrared properties of these objects. SUPERSCANPI processing evaluates the median flux for many different positions on the sky, resulting in an improvement in the effective sensitivity. A control sample consisting of objects with no Mg II absorption known at Zabs<1 but with the same distribution of absolute V-magnitude, Zem and radio-loud fraction for the background quasars was also processed. The Mg II sample was detected at 3{sigma} or better in all four IRAS bands with a significantly larger flux than the control sample at 60{mu}m and 100{mu}m. If this far-infrared emission is from the absorber galaxies, then the far-infrared luminosity of the composite Mg II absorber was found to be comparable to that of a starbursting galaxy, although such a high star-formation rate is inconsistent with the optical and near-infrared colors of low-redshift Mg II systems. Four of the quasars with individual IRAS detections have intervening galaxies identified with the Mg II absorption-lines. The spectral energy distributions of these galaxies imply far-infrared luminosities in excess of what Arp 220 would give at their redshifts. While all the external evidence suggests that the detection of far-infrared emission from the absorber sample may not be connected to the presence of the Mg II absorber, we discuss future observations which may help explain our results.
IRAS
Additional quasar in absorption-line (AL) sample, not in JHB (Cat. <J/ApJS/77/203>) Damped Ly{alpha} sample QSO Quasar name --- r_QSO Reference number=1 a : Steidel & Sargent (1992ApJS...80....1S) b : Aldcroft et al. (1994ApJS...93....1A) c : Lanzetta et al. (1991ApJS...77....1L) d : Junkkarinen et al. (1991, Cat. <J/ApJS/77/203>) e : White et al. (1993ApJ...407..456W) f : Turnshek et al. (1989ApJ...344..567T) g : Wolfe et al. (1986ApJS...61..249W) h : Francis & Hewitt (1993AJ....105.1633F) --- zem Emission redshift --- zabs Absorption redshift --- Vmag V magnitude from Hewitt & Burbidge (1993ApJS...87..451H) mag RL Radio loudness number=2 RL=log[f_v_(5GHz)/f_v_(V)], where f_v_(5GHz) is the radio flux density at 5GHz and [f_v_(V) is the V band flux density, based on 5 GHz flux densities from Veron-Cetty & Veron (1987, See Cat. VII/188) --- IRAS ADDSCAN detections BAL QSO's detected with IRAS ADDSCAN analysis QSO Quasar name --- Note Note number=1 c : galaxies or quasars in vicinity visible on Palomar Sky Survey. d : UGC 439, IRAS source is 45 arcseconds northwest of quasar. e : bright stars nearby visible on Palomar Sky Survey. f : IRAS source is 1 arcminute northwest of quasar. g : IRAS source is 30 arcseconds southeast of quasar. h : IRAS source is 1 arcminute north of quasar. i : NGC 3067, IRAS source is 2 arcminutes southwest of quasar. k : IRAS source is 1 arcminute south of quasar. l : NGC 6045. m : ESO 400-G012. --- zem Emission redshift --- Vmag V magnitude mag zabs Absorption redshift --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec l_S12um Limit flag on 12um --- S12um IRAS flux at 12um number=2 3 sigma upper limits given when not detected Jy e_S12um rms uncertainty on S12um Jy l_S25um Limit flag on 25um --- S25um IRAS flux at 25um number=2 3 sigma upper limits given when not detected Jy e_S25um rms uncertainty on S25um Jy l_S60um Limit flag on 60um number=2 3 sigma upper limits given when not detected --- S60um IRAS flux at 60um Jy e_S60um rms uncertainty on S60um Jy l_S100um Limit flag on 100um number=2 3 sigma upper limits given when not detected --- S100um IRAS flux at 100um Jy e_S100um rms uncertainty on S100um Jy RL Radio loudness number=3 RL=log[f_v_(5GHz)/f_v_(V)], where f_v_(5GHz) is the radio flux density at 5GHz and [f_v_(V) is the V band flux density, based on 5 GHz flux densities from Veron-Cetty & Veron (1987, See Cat. VII/188) unless otherwise stated. j : RL based on 5 GHz flux densities from Kellerman et al. (1994AJ....108.1163K). B : BL Lac O : OVV --- n_RL Note on RL number=3 RL=log[f_v_(5GHz)/f_v_(V)], where f_v_(5GHz) is the radio flux density at 5GHz and [f_v_(V) is the V band flux density, based on 5 GHz flux densities from Veron-Cetty & Veron (1987, See Cat. VII/188) unless otherwise stated. j : RL based on 5 GHz flux densities from Kellerman et al. (1994AJ....108.1163K). B : BL Lac O : OVV --- zabs2 Second absorption redshift --- zabs3 Second absorption redshift --- zabs4 Second absorption redshift --- zabs5 Second absorption redshift --- zabs6 Second absorption redshift --- zabs7 Second absorption redshift --- zabs8 Second absorption redshift --- zabs9 Second absorption redshift --- zabs10 Second absorption redshift --- Low redshift Mg II absorption line sample Control sample with no Mg II absorption for Zabs<1 QSO Quasar name --- n_QSO Note number=1 a: Objects with individual IRAS detections b: Removed for the control list for SUPERSCANPI without IRAS detections --- zem Emission redshift --- zabs Absorption redshift --- Vmag V magnitude mag RL Radio loudness --- Ref References, for table6 only number=2 1: Aldcroft et al. (1994ApJS...93....1A) 2: Steidel & Sargent (1992ApJS...80....1S) 3: Barthel et al. (1990A&AS...82..339B) --- James Marcout, Patricia Bauer CDS 1997 Jun 17 UNKNOWN UNKNOWN Prepared via OCR at CDS. In table6, for QSO 0736-0620, V=718.5 in the printed version, we change this value in 18.5 in the electronic table J_AJ_112_62.xml RR Lyrae variable stars in the CCD/Transit Instrument Survey J/AJ/112/742 J/AJ/112/742 Search for RR Lyrae Variables RR Lyrae variable stars in the CCD/Transit Instrument Survey C J Wetterer J T McGraw T R Hess R Grashuis Astron. J. 112 742 1996 1996AJ....112..742W Magnitudes Stars, variable We searched the CCD/Transit Instrument (CTI) survey databases for RR Lyrae variable stars. The CTI images a strip of the sky with a narrow spread of declination over all right ascensions. The resulting survey area covers a large range of both Galactic latitude and longitude, amounting to approximately 50deg^2. We detected a total of 42 RR Lyrae stars to a faint limiting magnitude of V=19. Thirty-four of these RR Lyae stars are newly discovered.
RR Lyrae final candidate list Star Star number --- RAh Right ascension (1987.5) h RAm Right ascension (1987.5) min RAs Right ascension (1987.5) s DEd Declination (1987.5) deg DEm Declination (1987.5) arcmin DEs Declination (1987.5) arcsec o_Bmag Total number of B observations --- o_Vmag Total number of V observations --- E(B-V) B-V colour excess mag Type RR Lyrae type number=1 RRab: type ab RR Lyrae RRc : type c RR Lyrae RRab(B): type ab RR Lyrae exhibiting Blazhko effect SX Phe: SX Phoenices type variable star W UMa: W Ursa Majoris or other eclipsing variable --- Note Note number=2 - : not discovered in search * : discovered in search + : discovered in <B-V> < 0.8 limit of first search --- Original V filter observational data Star Star number as in table1 --- HJD Heliocentric Julian Date number=1 Before JD 2449000 corresponds to CTI data, while after JD 2449000 corresponds to Capilla Peak data. d Vmag Instrumental V magnitude number=2 Instumental V magnitude of observation. Capilla Peak data has been transformed to CTI instrumental magnitudes. mag e_Vmag Error in instrumental V magnitude mag Patricia Bauer CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 14-Aug-1996 UNKNOWN UNKNOWN Table1 prepared via OCR at CDS. J_AJ_112_742.xml Scanned CCD V and I Photometry at the South Galactic Pole J/AJ/112/772 J/AJ/112/772 VI photometry in South Galactic Pole Scanned CCD V and I Photometry at the South Galactic Pole J A R Caldwell P L Schechter Astron. J. 112 772 1996 1996AJ....112..772C Galactic pole, south Photometry, CCD The tables described below correspond to tables I-VII as mentioned in sections 5 and 6 of the printed paper. Catalogs of V and I photometry for two 20 square degree regions near the South Galactic Pole, containing 30,000 and 19,000 stars, have been constructed using a CCD in time delay integration mode. Internal and external comparisons indicate a characteristic photometric accuracy ranging from 0.02mag at V~12 to 0.05 at V~18-18.5.
Catalog CS1 of CCD scanning photometry at the SGP Catalog CS2 of CCD scanning photometry at the SGP CS CS star number (CS1 for table1; CS2 for table2) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vmag V magnitude mag Imag I magnitude mag V-I V-I color index mag Code Four-digit code including number of V,I values A four-digit number gives from left to right: a first digit of 1 or 0 depending on whether or not the star was found to be a split star on any scan, a second digit for the number of V values, a third digit for the number of I values, and a last digit for the number of nearly simultaneous V and I values. --- e_Vmag V magnitude error mag e_Imag I magnitude error mag e_V-I V-I color error mag S s = split stars A split star has at least some contributory data where another star was sufficiently close that the "split star" method of solution (Schechter et al, 1993PASP..105.1342S) was invoked. --- U u = uncertainty because star is faint A "u" appears for stars so faint that the nonlinearity correction (Section 4 of the printed paper) was excessively uncertain. These were excluded from all use and are thus not included in the totals given in Table 2 of the printed paper. --- Comparison with Eriksson, 1978UppOR..11....1E CS1 CS1 star number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vcs CS V magnitude mag Ics CS I magnitude mag Ne Eriksson (1978UppOR..11....1E) number --- Ve Eriksson (1978UppOR..11....1E) V magnitude mag B-Ve Eriksson (1978UppOR..11....1E) B-V color mag U-Be Eriksson (1978UppOR..11....1E) U-B color mag Ve-Vcs Eriksson - CS V magnitude difference Median (53 pts, 2 rej)=0.000+/-0.003, Median-based est. std. dev.=0.015 mag Comparison with Reid and Gilmore, 1982MNRAS.201...73R, Appendix A (p. 93) CS1 CS1 star number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vcs CS V magnitude mag Ics CS I magnitude mag Nr Reid & Gilmore App. A number Reid and Gilmore, 1982MNRAS.201...73R, Appendix A (p. 93) --- Vr Reid & Gilmore App. A V magnitude mag B-Vr Reid & Gilmore App. A B-V color mag V-Rr Reid & Gilmore App. A V-R color mag Ir Reid & Gilmore App. A I magnitude mag Vr-Vcs R&G - CS V magnitude difference Median (25 pts, 5 rej)=0.006+/-0.005, Median-based est. std. dev.=0.020 mag Ir-Ics R&G - CS I magnitude difference Median (40 pts, 4 rej)=0.012+/-0.005, Median-based est. std. dev.=0.024 mag Comparison with Reid and Gilmore, 1982MNRAS.201...73R, Table 7 (p. 87) CS1 CS1 star number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vcs CS V magnitude mag Ics CS I magnitude mag Nr Reid & Gilmore Tab. 7 number Reid and Gilmore, 1982MNRAS.201...73R, Table 7 (p. 87) --- Vr Reid & Gilmore Tab. 7 V magnitude mag Ir Reid & Gilmore Tab. 7 I magnitude mag Vr-Vcs R&G - CS V magnitude difference Median (32 pts)=-0.031+/-0.010, Median-based est. std. dev.=0.046 mag Ir-Ics R&G - CS I magnitude difference Median (29 pts, 2 rej)=-0.017+/-0.011, Median-based est. std. dev.=0.047 mag Comparison with Murray-Argyle-Corben, 1986MNRAS.223..629M (Cat. <I/129>) CS1 CS1 star number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vcs CS V magnitude mag Ics CS I magnitude mag Nco Corben number Murray, Argyle and Corben, 1986MNRAS.223..629M (Cat. <I/129>) --- Vco Corben V magnitude mag B-Vco Corben B-V color mag V-Rco Corben (Cat. <I/129>) V-R color mag Ico Corben (Cat. <I/129>) I magnitude mag Vco-Vcs Corben - CS V magnitude difference Median (42 pts)=-0.004+/-0.004, Median-based est. std. dev.=0.019 mag Ico-Ics Corben - CS I magnitude difference Median (73 pts)=-0.002+/-0.001, Median-based est. std. dev.=0.010 mag Comparison of Stars with Multiple CCD/Photoelectric Photometry CS1 CS1 star number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Src Source Source Key: ccd photometry: CS this work Tab. 1 p.e.photometry: Ca this work Tab. 4 Co Murray-Argyle-Corben (Cat. <I/129>) Er Eriksson (1978UppOR..11....1E) RA Reid-Gilmore (1982MNRAS.201...73R, App. A) R7 Reid-Gilmore (1982MNRAS.201...73R, Tab. 7) ptg.photometry: Ep Eriksson (1978UppOR..11....1E) KG Kuijken-Gilmore (1989MNRAS.239..605K) --- Vmag V magnitude mag Imag I magnitude mag CDS 1997 Jan 30 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 14-Aug-1996 J_AJ_112_772.xml Stellar Populations in the Dwarf Elliptical Galaxy NGC 147 J/AJ/113/1001 J/AJ/113/1001 Stellar photometry in NGC 147 Stellar Populations in the Dwarf Elliptical Galaxy NGC 147 M Han J G Hoessel J S Gallagher III J Holtzman P B Stetson J Trauger G E Ballester C Burrows J Clarke D Crisp R Griffiths C Grillmair J Hester J Krist J R Mould P Scowen K Stapelfeldt A Watson J Westphal Astron. J. 113 1001 1997 1997AJ....113.1001H Galaxies, photometry Deep V and I CCD images in a central and an outer field of the Local Group dwarf elliptical galaxy NGC 147 have been obtained with the Wide Field and Planetary Camera-2 (WFPC2) on board of the Hubble Space Telescope. The color-magnitude diagram shows a number of interesting features, including a well defined red giant branch (RGB), a red horizontal branch (HB), a strong red clump, and a small number of extended asymptotic giant branch (EAGB) stars. A mean distance modulus of (m-M)_0_=24.39 is derived based on both the HB and the RGB tip brightness. The metallicity [Fe/H] as determined from the RGB color has a mean value of -0.91 in the central field, and -1.0 in the outer field; and the outer field shows a weak tendency of increasing metallicity with galactocentric radius. A metallicity dispersion is also present in the galaxy, and it shows a clear radial variation in the sense that a larger dispersion is seen at smaller radii. The small population of EAGB stars indicates the presence of intermediate-aged (several Gyr) stars in the galaxy, while the absence of the main sequence stars with M_V_<1 shows that star formation ceased at least 1 Gyr ago. The distribution of the EAGB stars indicates that the younger stars are more centrally concentrated than the majority of older stars. A similar age gradient is also implied by the relative distribution of the HB stars, which appear to be more populous at larger radii. These results are considered within the context of theoretical models for the evolution of dwarf elliptical galaxies. (Copyright) 1997 American Astronomical Society.
HST NGC 147 00 33.1 +48 31
NGC 147 - inner field photometry NGC 147 - outer field photometry Xpos X pixel coordinate The coordinate system is defined by simply stacking up the contiguous fields of the 4 chips in each field (see HST/WFPC2 Handbook v3.0), and defining the central joining point to be at (800,800). X and Y are in units of WF pixels. North is up, East left. pix Ypos Y pixel coordinate pix Vmag V magnitude mag e_Vmag Error in Vmag mag Imag I magnitude mag e_Imag Error in Imag mag CDS 1997 Jul 04 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 09-Apr-1997 J_AJ_113_1001.xml UIT: Ultraviolet Observations of the Small Magellanic Cloud J/AJ/113/1011 J/AJ/113/1011 UV Observations of the SMC UIT: Ultraviolet Observations of the Small Magellanic Cloud R H Cornett M R Greason J K Hill J W Parker W H Waller R C Bohlin K -P Cheng S G Neff R W O'Connell M S Roberts A M Smith T P Stecher Astron. J. 113 1011 1997 1997AJ....113.1011C Magellanic Clouds Photometry, ultraviolet The table data were referred to, but did not appear in, the printed paper. A mosaic of four UIT (Ultraviolet Imaging Telescope) far-UV (FUV) ({lambda}_(eff)_=1620{AA}) images, with derived stellar and H II region photometry, is presented for most of the Bar of the SMC. The UV morphology of the SMC's Bar shows that recent star formation there has left striking features including: (a) four concentrations of UV-bright stars spread from northeast to southwest at nearly equal (~30arcmin=0.5kpc) spacings; (b) one of the concentrations, near DEM 55, comprises a well-defined 8-arcmin diameter ring surrounded by a larger H{alpha} ring, suggestive of sequential star formation. FUV PSF photometry is obtained for 11,306 stars in the FUV images, resulting in magnitudes m(162). We present a FUV luminosity function for the SMC Bar, complete to m(162)~14.5. Detected objects are well correlated with other SMC Population I material; of 711 H{alpha} emission-line stars and small nebulae within the UIT fields of view, 520 are identified with FUV sources. The FUV photometry is compared with available ground-based catalogs of supergiants, yielding 191 detections of 195 supergiants with spectral type earlier than F0 in the UIT fields. The (m(162)-V) color for supergiants is a sensitive measure of spectral type. The bluest observed colors for each type agree well with colors computed from unreddened Galactic spectral atlas stars for types earlier than about A0; for later spectral types the observed SMC stars range significantly bluer, as predicted by comparison of low-metallicity and Galactic-composition models. Redder colors for some stars of all spectral types are attributed to the strong FUV extinction arising from even small amounts of SMC dust. Internal SMC reddenings are determined for all catalog stars. All stars with E(B-V)>0.15 are within regions of visible H{alpha} emission. FUV photometry for 42 H{alpha} -selected H II regions in the SMC Bar is obtained for stars and for total emission (as measured in H II-region-sized apertures). The flux-weighted average ratio of total to stellar FUV flux is 2.15; consideration of the stellar FUV luminosity function indicates that most of the excess total flux is due to scattered FUV radiation, rather than stars fainter than m(162)=14.5. Both stellar and total emission are well correlated with H{alpha} fluxes measured by Kennicutt and Hodge (1986ApJ...306..130K), yielding FUV/H{alpha} flux ratios that are consistent with models of SMC metallicity, ages from 1-5Myr, and moderate (E(B-V)=0.0-0.1mag) internal SMC extinction. (Copyright) 1997 American Astronomical Society.
ASTRO 1/UIT
UIT FUV magnitudes of 11306 stars Star UIT star number --- Field UIT field number Fields are 40 arcmin in diameter; locations of Fields 1, 2, 3, and 4 are shown in the printed paper. --- Xpos X pixel coordinate 1 pix = 1.12 arcsec; North is up, East left pix Ypos Y pixel coordinate pix RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) Mean uncertainty in UIT positions is approximately 5 arcsec, with smaller values near field centers (X=1023.5, Y=1023.5) and larger values near the edges. s DE- Sign declination --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec m162 m(162) derived from PSF photometry UIT magnitudes are defined by m({lambda})=-2.5 log(F({lambda})) - 21.1 where F({lambda}) is in units of ergs/cm^2^/Angstrom/s (mW/m^2^/Angstrom) and is the mean flux per Angstrom over the UIT bandpass. The magnitudes in this table are made with UIT's 'B5' bandpass, which has an effective wavelength (for a flat input spectrum) of 1620 Angstroms, and an effective width of 225 Angstroms. These magnitudes are termed 'm(162)' (and occasionally 'm(B5)') in the literature. More details on UIT hardware, observations, and data reduction are in Stecher et al. (1992ApJ...395L...1S) and in Stecher et al. (1997PASP..109..584S). mag e_m162 Estimated error in m162 This is the uncertainty returned by UITPHOT, an IDL/UIT implementation of DAOPHOT which incorporates the noise characteristics of UIT. It includes sky and other photometric uncertainties, but no absolute calibration uncertainty. From comparison with IUE spectra, the uncertainty in the absolute calibration is about 0.15 for typical stars in this table. mag CDS 1997 Jul 04 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 09-Apr-1997 J_AJ_113_1011.xml Fabry-Perot Observations of Globular Clusters. III. M15 J/AJ/113/1026 J/AJ/113/1026 Fabry-Perot Observations of M15 Fabry-Perot Observations of Globular Clusters. III. M15 K Gebhardt C Pryor T B Williams J E Hesser P B Stetson Astron. J. 113 1026 1997 1997AJ....113.1026G J/AJ/110/1699 : Paper II. (47 Tuc, NGC 6397 & M30) (Gebhardt+ 1995) J/ApJ/347/251 : Dynamics of Globular Cluster M15 (Peterson+ 1989) Pryor et al., Paper I. 1993BAAS...25Q1406P Clusters, globular Radial velocities We have used an Imaging Fabry-Perot Spectrophotometer with the Sub-arcsecond Imaging Spectrograph on the Canada-France-Hawaii Telescope to measure velocities for 1534 stars in the globular cluster M15 (NGC 7078) with uncertainties between 0.5 and 10km/s. Combined with previous velocity samples, the total number of stars with measured velocities in M15 is 1597. An average seeing of 0.8" allowed us to obtain velocities for 144 stars within 10" of the center of M15, including 12 stars within 2". The velocity dispersion profile for M15 remains flat at a value of 11km/s from a radius of 0.4 into our innermost reliable point at 0.02 (0.06pc). Assuming an isotropic velocity dispersion tensor, this profile and the previously-published surface brightness profile can be equally well represented either by a stellar population whose M/L varies with radius from 1.7 in solar units at large radii to 3 in the central region, or by a population with a constant M/L of 1.7 and a central black hole of 1000M_{sun}_. A non-parametric mass model that assumes no black hole, no rotation, and isotropy constrains the mass density of M15 to better than 30% at a radius of 0.07 parsecs. The mass-density profile of this model is well represented by a power law with an exponent of -2.2, the value predicted by models of cluster core-collapse. Using the assumption of local thermodynamic equilibrium, we estimate the present-day mass function and infer a significant number of 0.6-0.7 M_{sun}_ objects in the central few parsecs, 85% of which may be in the form of stellar remnants. Not only do we detect rotation; we find that the position angle of the projected rotation axis in the central 10" is 100deg different from that of the whole sample. We also detect an increase in the amplitude of the rotation at small radii. Although this increase needs to be confirmed with better-seeing data, it may be the result of a central mass concentration. (Copyright) 1997 American Astronomical Society.
M 15 NGC 7078 21 29 58.3 +12 10 00
Velocity data ID Star identification --- Xpos X offset from cluster center (E through N) The cluster center coordinates are given in Guhathakutra et al. 1996AJ....111..267G arcsec Ypos Y offset from cluster center (E through N) arcsec Vel Mean velocity km/s e_Vel Uncertainty in Vel km/s V(FP) Fabry-Perot magnitude Fabry-Perot magnitude, estimated from the fitted continuum of the authors' 3 Angstrom spectrum. mag Prob Probability of the chi-square The probability of the chi-square from the multiple measurements exceeding the observed value -- a low probability suggests a variable velocity -- or a note. % Note Note A note of 'bias' indicates the star is beyond the unbiased radius and is not used in the dynamical analysis. A note of 'non' indicates the star was determined to be a non-member based on its radial velocity. --- Repeat measurements ID Star identification --- CFHT95 Velocity from the 1995 CFHT data km/s e_CFHT95 Uncertainty in CFHT95 km/s CFHT94 Velocity from the 1994 CFHT data km/s e_CFHT94 Uncertainty in CFHT94 km/s FP92 Velocity from 1992 CTIO data (paper I, Pryor et al., 1993BAAS...25Q1406P) km/s e_FP92 Uncertainty in FP92 km/s FP91 Velocity from 1991 CTIO data (paper I, Pryor et al., 1993BAAS...25Q1406P) km/s e_FP91 Uncertainty in FP91 km/s PSC Velocity from Peterson et al. (1989) (Cat. <J/ApJ/347/251>) km/s e_PSC Uncertainty in PSC km/s table1.tex AASTeX version of table1.dat table2.tex AASTeX version of table2.dat CDS 1997 Jul 04 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 09-Apr-1997 J_AJ_113_1026.xml The age of NGC 3680 and a test of convective overshoot. J/AJ/113/1045 J/AJ/113/1045 BV photometry of NGC 3680 The age of NGC 3680 and a test of convective overshoot. V Kozhurina-Platais P Demarque I Platais J A Orosz S Barnes Astron. J. 113 1045 1997 1997AJ....113.1045K I/212 : Proper motions in NGC 3680 (Kozhurina-Platais+, 1995) J/A+AS/118/407 : NGC 3680 CCD photometry & velocities (Nordstroem+ 1996) J/A+A/322/460 : NGC 3680 photometry and radial velocities (Nordstrom+ 1997) Clusters, open Photometry, CCD A new CCD BV color-magnitude diagram (CMD) has been derived for the intermediate age open cluster NGC 3680. The quality of photometry coupled with the best-to-date knowledge of cluster memberships allows for a detailed isochrone fit to the CMD. The theoretical isochrones have been constructed using the Yale Rotating Evolution Code (YREC) in its non-rotating mode and the OPAL opacities (circa 1991). Four sets of isochrones have been calculated: one for the standard stellar model calibrated to the Sun and three others for models with different amounts of convective overshoot at the edge of the convective core, namely, 0.15, 0.20, and 0.25H_p_, where H_p_ is the pressure scale height at the core edge. All four sets of theoretical isochrones were adjusted to an adopted distance modulus of V_0_-M_V_=10.20 and reddening E(B-V)=0.075 which leads to ages of 1.3+/-0.15, 1.5+/-0.15, 1.6+/-0.15, and 1.7+/-0.15Gyr, respectively The uncertainties in age mainly reflect a subjective decision in differentiating a good fit from a poorer one The model with a convective overshoot of 0.20H_p_ seems to yield the best fit to the sharply curved upper main sequence. Hence, the estimated age of NGC 3680 is 1.6+/-0.15Gyr. The adopted overshoot parameter ostensibly is uncertain by +/-0.05H_p_. For comparison, the same stellar models with overshoot of 0.25H_p_ were fit to the color-magnitude diagram of the cluster NGC 752, which is similar in age and composition to NGC 3680 The age estimate for NGC 752 is 1.6+/-0.2Gyr, assuming V_0_-M_V_=8.20 and E(B-V)=0.030 for the cluster.
The BV CCD photometry for probable cluster stars in NGC 3680 Star Star number --- m_Star Multiplicity index on Star number --- n_Star Note on Star number=1 a : B, V-photometry from other studies (see Sec. 2.2). b : Adopted binaries (see Sec. 3.2). --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag B-V B-V magnitude mag e_Vmag rms uncertainty on Vmag mag e_Bmag rms uncertainty on Bmag mag o_Vmag Number of individual CCD observations --- Member Proper motion membership probability % James Marcout, Patricia Bauer CDS 1997 Oct 03 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_113_1045.xml Chemical Abundances of Galactic Cepheid Variables That Calibrate the P-L Relation J/AJ/113/1073 J/AJ/113/1073 Abundances in Cepheid Variables Chemical Abundances of Galactic Cepheid Variables That Calibrate the P-L Relation A M Fry B W Carney Astron. J. 113 1073 1997 1997AJ....113.1073F Equivalent widths Stars, variable We have completed spectroscopic studies of 23 Galactic cepheids to determine possible metallicity effects on measuring the zero point of the P-L relation. We find a spread of 0.4dex in [Fe/H], which is not the result of either observational scatter or of a metallicity gradient within the Galactic disk. We find a smaller, less significant spread of 0.2dex in [{alpha}/Fe]. Our results are robust, determined by constancy of [Fe/H] derived at differing temperatures throughout the pulsational cycle, and abundances of two dwarfs compared to U Sgr in the cluster M25. We discuss briefly the effect of metallicity on the P-L relation. We also argue that EV Sct and QZ Nor are overtone pulsators, and that the latter is not a member of the cluster NGC 6067. (Copyright) 1997 American Astronomical Society.
Equivalent widths of Fe I and Fe II Equivalent widths of Alpha-peak elements Name Star name --- phi Phase --- lambda Line wavelength 0.1nm EW Equivalent width 0.1pm Ion Ion designation --- log(gf) log of oscillator strength --- Chi Chi value eV table2.tex AASTeX version of Tables 2a to 2o table3.tex AASTeX version of Tables 3a to 3d Patricia Bauer CDS 1997 Jul 04 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 10-Apr-1997 J_AJ_113_1073.xml Ultraviolet Photometry of Stars in the Compact Cluster R136 in the Large Magellanic Cloud J/AJ/113/1691 J/AJ/113/1691 Stars in R136 Ultraviolet Photometry of Stars in the Compact Cluster R136 in the Large Magellanic Cloud D A Hunter W D Vacca P Massey R Lynds E J O'Neil Astron. J. 113 1691 1997 1997AJ....113.1691H Photometry, ultraviolet We present ultraviolet photometry of stars in the Large Magellanic Cloud star cluster R136. The data were obtained with the refurbished Wide Field/Planetary Camera on the Hubble Space Telescope through an ultraviolet filter centered at 1750A (F170W). These data, combined with optical HST observations presented previously, are used to explore the hot, luminous stellar population within the cluster. The first question we wanted to address was whether the ultraviolet could place better constraints on differential reddening and the degree of coevality within the cluster than optical photometry alone. The stellar sequence in the color magnitude diagram using the F170W-F555W color is broader than it was in the optical and is broader than would be expected from photometric uncertainties. Although there could be a modest age spread among the massive stars, a large part of the intrinsic spread in the color-magnitude diagram is likely to be due to reddening differences. There is also some evidence that stars in the outer parts of the cluster are affected by a larger range in reddening than those in the smaller region of the cluster core. The second question we addressed is whether ultraviolet photometry in combination with optical photometry can distinguish the most massive stars more readily than is possible with the optical colors. The F170W-F555W color is better at separating B supergiants, of which there is only one in R136, from comparably bright O and Wolf-Rayet stars. However, spectral classifications of the stars within R136 will be necessary to properly identify stellar types of the rest of the stars and to disentangle age and reddening effects. (Copyright) 1997 American Astronomical Society.
HST R 136 RMC 136 HD 38268 05 38 42.8 -69 06 03
The cluster photometry Star Star identification number --- Xpos X pixel coordinate pix Ypos Y pixel coordinate pix F170W F170W magnitude mag e_F170W Error in F170W mag F555W F555W magnitude mag e_F555W Error in F555W mag F170W-F555W F170W-F555W color mag e_F170W-F555W Error in F170W-F555W mag F336W-F555W F336W-F555W color mag e_F336W-F555W Error in F336W-F555W mag CDS 1997 Jul 04 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 02-May-1997 J_AJ_113_1691.xml The structure of the light curves of the RR Lyrae variables in the Oosterhoff type I cluster NGC 6171 J/AJ/113/1711 J/AJ/113/1711 RR Lyrae in NGC 6171 The structure of the light curves of the RR Lyrae variables in the Oosterhoff type I cluster NGC 6171 C M Clement I Shelton Astron. J. 113 1711 1997 1997AJ....113.1711C Clusters, globular Magnitudes Stars, variable The complete table caption from the printed paper follows: The Julian dates represent the time of mid-exposure. The magnitudes are on the standard V system. There are observations for 16 stars included here. They are variables: 4, 6, 7, 8, 9, 10, 12, 14, 15, 17, 18, 19, 20, 21, 23 and 24 (Cl* NGC 6171 DICK VNN, NN = 1 to 24, in Simbad database). CCD observations have been used to derive precise light curves and Fourier parameters for sixteen RR Lyrae variables in the Oosterhoff type I globular cluster NGC 6171. It is found that, for the RRab stars, the Fourier phase differences {phi}_21_, {phi}_31_ and {phi}_41_ all correlate with period, but the amplitude ratios R_21_, R_31_, and R_41_ do not. For the RRc stars, R_21_, {phi}_31_, and {phi}_41_ correlate with period, but {phi}_21_, R_31_, and R_41_ do not. It is also found that a plot of R_21_ against {phi}_21_ is a useful tool for distinguishing between RRc and RRab stars, regardless of color or chemical composition. Simon's method that relates physical properties of RRc stars to the pulsation period and Fourier phase parameter {phi}_31_ has been used to determine the mass, luminosity, temperature and a helium parameter for the RRc stars. A comparison with the parameters determined from CCD observations of RRc stars in six other galactic globular clusters indicates that mean masses and mean luminosities increase and mean temperatures and helium abundances decrease with decreasing cluster metal abundance. The formulae of Jurcsik & Kovacs (1996, Cat. <J/A+A/312/111>) for relating Fourier parameters of RRab stars to [Fe/H] and luminosity have been tested and the results are reasonable. (c) 1997 American Astronomical Society.
NGC 6171 M 107 C 1629-129 16 32 31.8 -13 03 13
Las Campanas observations for NGC 6171 Vname Variable name, as in Dickens, (1970ApJS...22..249D) Cl* NGC 677 DICK in Simbad --- JD Julian date JD Vmag V magnitude mag CDS 1998 Feb 04 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 30-Oct-1997 J_AJ_113_1711.xml On the stellar population and star-forming history of the Orion Nebula Cluster J/AJ/113/1733 J/AJ/113/1733 Orion Nebula Cluster population On the stellar population and star-forming history of the Orion Nebula Cluster L A Hillenbrand Astron. J. 113 1733 1997 1997AJ....113.1733H II/171 : Parenago Catalog of Stars in Orion Nebula (Parenago 1954) Photometry, Cousins Populations, stellar We report on the first phase of a study of the stellar population comprising the Orion Nebula Cluster (ONC). Approximately 50% of the ~3500 stars identified to date within ~2.5pc of the namesake Trapezium stars are optically visible, and in this paper we focus on that sample with I<2.5mag. The large number and number density of stars (n_peak_>10^4^pc^-3^), the wide range in the stellar mass (~0.1-50M_{sun}_), and the extreme youth (<1-2Myr) of the stellar population, make the ONC the best site for investigating: (1) the detailed shape of a truly "initial" mass spectrum; (2) the apparent age spread in a region thought to have undergone triggered star formation; (3) the time sequence of star formation as a function of stellar mass; and (4) trends of all of the above with cluster radius.
Optical properties of ONC stars ID Identification number number=1 ID = adopted ``red'' identification number: 1-1053 from Jones & Walker, 1988AJ.....95.1755J 1054-2999 from Parenago, 1954, Cat <II/171> 3000-3999 from this paper, 1993 January CCD data 5000-5999 from this paper, 1995 January CCD data 6000-6999 from this paper, 1996 January CCD data 9000-9999 from Prosser et al., 1994ApJ...421..517P (number is 9000 plus original number from that paper) --- m_ID Multiplicity index on ID --- Parenago Parenago (1954, Cat <II/171>) number number=2 Par = Parenago or ``blue'' identification number --- Mem =-9 Membership probability number=3 Adopted membership probability taken from Jones & Walker (1988AJ.....95.1755J) with first priority, and supplemented with van Altena et al. (1988AJ.....95.1744), McNamara (1976AJ.....81..375M and 1976AJ.....81..845M), McNamara & Huels (1983A&AS...54..221M), or McNamara et al. (1989AJ.....97.1427M). In addition, sources showing proper motion on my CCD frames were given a membership probability of "0" while sources designated as "proplyds" were given a membership probability of 99%; see "Comm" column. % RAh Right ascension (2000) number=4 Equinox 2000. position, referenced to the HST Guide Star Catalog (Cat. <I/220>; see text. h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Rproj Projected radius from Theta 1C Ori min Imag =-9.99 Adopted I magnitude (Cousins) mag l_V-I Limit flag on V-I (from Prosser et al., 1994ApJ...421..517P) --- V-I =-9.99 Adopted V-I color index mag Ref Photometry reference number=5 Ref = photometry reference: (1) this paper; 1993 January CCD data (2) this paper; 1995 February CCD data (3) this paper; 1996 February CCD data (4) Prosser et al., 1994ApJ...421..517P (5) Jones & Walker, 1988AJ.....95.1755J (6) McCullough et al., 1995ApJ...438..394M (7) Breger, Gehrz, & Hackwell, 1981ApJ...248..963B (8) Penston, 1973ApJ...183..505P or Penston et al., 1975MNRAS.171..219P (9) Herbig & Terndrup, 1986ApJ...307..609H (10) Herbst, 1993, priv. comm. (11) Rydgren & Vrba, 1984AJ.....89..399R --- Comm Comment reference number=6 Comm = comment: (1) externally ionized "proplyd" (2) nebulous on 0.9m CCD images (3) unresolved double on 0.9m CCD images (4) >1.5 mag variability at I-band compared to Jones & Walker (1988AJ.....95.1755J) photographic photometry, or as designated by Choi & Herbst (1996AJ....111..283C) or by Jones & Walker (1988AJ.....95.1755J) (5) alternate designation from Prosser et al. (1994ApJ...421..517P): JW378a = 9011, JW378b = 9012, JW377a = 9013, JW377b = 9014, JW399a = 9034, JW399b = 9033, JW435a = 9057, JW435b = 9058, JW436a = 9059, JW436b = 9060, JW445b = 9067, JW445a = 9068, JW472a = 9099, JW472b = 9098, JW484a = 9111, JW484b = 9112, JW504b = 9125, JW504a = 9126, JW509a = 9129, JW509b = 9130, JW511b = 9134, JW511a = 9136, JW519b = 9143, JW519a = 9144, JW526b = 9150, JW526a = 9152, JW551b = 9172, JW551a = 9173, JW552a = 9183, JW552b = 9184, JW553a = 9185, JW553b = 9186, JW570a = 9202, JW570b = 9203, JW598b = 9234, JW598a = 9235, JW648b = 9262, JW648a = 9263, JW687b = 9286, JW687a = 9288, JW748b = 9314, JW748a = 9315, JW766b = 9321, JW766a = 9322, JW776a = 9323, JW776b = 9324 (6) coordinates for JW618 given by Jones & Walker are incorrect; source is NE of their position (7) source has close companion in infrared images (8) large proper motion on 0.9m CCD frames; assigned zero membership probability (9) resolved double on 0.9m CCD frames --- logT =-9.999 Effective temperature of adopted spectral type [K] SpT Spectral type with reference in parentheses number=7 Spectral Type = all available spectral type information with references in parentheses as listed below. B = Blanco, 1963ApJ...137..513B CK = Cohen & Kuhi, 1979ApJS...41..743C D = Duncan, 1993ApJ...406..172D Eetal = Edwards et al., 1993AJ....106..372E GS = Greenstein & Struve, 1946PASP...58..366G H = Hillenbrand, 1997 (this paper) "e" indicates emission in the CaII triplet lines "<" indicates spectral type is earlier than that listed ">" indicates spectral type is later than that listed -- most spectra later than ~M3 show indications of surface gravity intermediate between that of dwarfs and giants, especially longward of 8000{AA} Ham = C. Hamilton, 1994 unpublished masters thesis Her = Herbig, quoted in Walker, 1969ApJ...155..447W HP = Herbig, private communication, 1996 HT = Herbig & Terndrup, 1986ApJ...307..609H or reference therein J = Johnson, 1965ApJ...142..964J LA = Levato & Abt, 1976PASP...88..712L or Abt & Levato, 1977PASP...89..797A LDW = Lallemand, Duchesne, & Walker, 1960PASP...72..268L M = McNamara, 1976AJ.....81..375M and 1976AJ.....81..845M P = Prosser & Stauffer, unpublished Par = Parenago, 1954, Cat. <II/171> Petal = Penston, Hunter, & O'Neill, 1975MNRAS.171..219P or Penston, 1973ApJ...183..505P S = Strand, 1958 reference (mostly to Sharpless) Sam = A.E. Samuel, 1993 unpublished PhD thesis SBB = Smith, Beckers, & Barden, 1983ApJ...271..237S T = Trumpler, 1931PASP...43..255T vA = van Altena et al., 1988AJ.....95.1744 W = Walker, 1983ApJ...271..642W WSH = Wolff, Strom, & Hillenbrand, 1998, in prep. --- Derived properties of ONC stars ID Adopted identification number --- m_ID Multiplicity index on ID --- AV =-9.99 Visual extinction number=1 Visual extinction calculated from optical photometry and spectral type; values of 0.00 indicate that the V-I_C_ color is too blue for the spectral type. mag log(Teff) =-9.99 Effective temperature assigned from spectral type [K] log(L) =-9.99 Stellar luminosity number=2 Stellar luminosity calculated from application of a bolometric correction to reddening-corrected photometry, assuming a distance of 470pc; see Table 1 for applicable cluster membership information. luminosities are lower limits in cases where A_V_=0.0. [solLum] R =-9.99 Stellar radius calculated from luminosity and effective temperature solRad M =-9.99 Stellar mass number=3 Stellar mass interpolated from D'Antona & Mazitelli (1994ApJS...90..467D) tracks for stars <3M_{sun}_, from Swenson et al. (1994ApJ...425..286S) tracks for stars 3-5M_{sun}_, and from the ZAMS mass-luminosity relationship for stars >5M_{sun}_. solMass log(age) =-9.99 Stellar age interpolated from D'Antona & Mazitelli (1994ApJS...90..467D) isochrones [yr] Patricia Bauer CDS 1998 Aug 04 Lynne Hillenbrand <lah@astro.caltech.edu> J_AJ_113_1733.xml A Near-Infrared Imaging Survey of NGC 2282 J/AJ/113/1788 J/AJ/113/1788 Near-IR Imaging Survey of NGC 2282 A Near-Infrared Imaging Survey of NGC 2282 D J Horner E A Lada C J Lada Astron. J. 113 1788 1997 1997AJ....113.1788H Nebulae Photometry, infrared We present the first near-infrared (JHK) imaging and photometry of a young cluster associated with NGC 2282, a reflection nebula in Monoceros. Our observations reveal that the cluster is centrally concentrated with a surface density that falls as 1/r. The cluster has a radius of roughly 1.6 pc and contains at least 100 members, approximately 9% of which exhibit infrared excess emission characteristic of young stellar objects. Infrared extinction maps suggest that the cluster is located at the edge of a molecular cloud and is not heavily reddened. We construct the K-band luminosity function (KLF) of the cluster and find that it increases with magnitude up to the completeness limit of our observations (m_(K)=15.0). The shape of the KLF is similar to those of other young clusters, such as IC 348 and the Trapezium, which suggest that the cluster contains a significant population of pre-main sequence stars. However, at the distance of NGC 2282 (1.7kpc) our observations are not deep enough to sample the low mass end of the cluster IMF. Consequently, our KLF does not provide meaningful constraints on either the age of the cluster or the duration of star formation within it. On the other hand, the low extinction toward the cluster, its location at the edge of a molecular cloud, and the relatively small fraction of infrared excess sources suggest that it is a relatively evolved cluster of pre-main-sequence stars with an age of 5-10x10^6^ years. (Copyright) 1997 American Astronomical Society. For a description of the JHK photometric system, see e.g. <GCPD/09>
1995 1.5 meter telescope CIRIM data Num Source number --- Note Note flag a - Source 137: nebulous object A b - Source 177: HD 289120, the central star illuminating the reflection nebula c - Source 275: nebulous object B/EQ 0644.3+0121 d - Source 295: nebulous object C e - Source 314: nebulous object D f - Source 328: V507 Mon, spectroscopic binary --- RAh Right ascension, J2000 h RAm Right ascension, J2000 min RAs Right ascension, J2000 s DE- Sign of Declination, J2000 --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec Jmag J magnitude (1.20{mu}m) No color correction has been applied to the J-band magnitudes. mag e_Jmag Error in Jmag mag Hmag H magnitude (1.62{mu}m) mag e_Hmag Error in Hmag mag Kmag K magnitude (2.20{mu}m) mag e_Kmag Error in Kmag mag table3.tex AASTeX version of table3.dat CDS 1997 Jul 04 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 02-May-1997 J_AJ_113_1788.xml A VLA survey of the Hercules cluster. I. The H I data J/AJ/113/1939 J/AJ/113/1939 VLA Survey of Hercules cluster. I. A VLA survey of the Hercules cluster. I. The H I data J M Dickey Astron. J. 113 1939 1997 1997AJ....113.1939D Clusters, galaxy H I data The channel maps for the Hercules cluster are stored in 63 Encapsulated Postscript files named fig36.eps, fig37.eps, ... fig98.eps. For all figures, the contour levels are as in figure 15 in the printed paper. This paper presents results from a survey of lambda 21-cm emission from galaxies in the Hercules cluster, A2151 and A2147. Four VLA primary beam areas were covered, a total area of 0.9 square degrees, including some 120 spiral galaxies brighter than 17.5m. The velocity resolution is 44km/s, the angular resolution 25". The detection threshold at field center is 2.6x10^8 h^{-2}M_{sun}_ in H I mass or about 1.8x10^20cm^-2^ in column density. There are 61 galaxies detected in H I, of which about 25 had been previously detected at lambda 21-cm. About ten of the detections correspond to galaxies that are very faint in the optical, m_E_>=18 or M>=-17mag-5logh. Some of these low surface brightness galaxies have very extended H I disks, with r>=15kpc. The abundance of H I is a strong function of position in the cluster, with galaxies in the south and west showing hardly any gas, and galaxies in the north and east of A2151 frequently having massive, extended gas disks. The morphology of the remnants of gas in galaxies in the south and west suggests that the intracluster medium is responsible for their H I deficiency, but there are also several dramatic galaxy mergers in progress. (c) 1997 American Astronomical Society.
ACO 2151 Hercules cluster 16 05.2 +17 45 ACO 2147 16 02.3 +15 55
Galaxies detected in H I File Name of the file in eps sub-directory --- Alias Galaxy alias number=1 Fields 'ne' (northeast), 'ce' (center), and 'sw' (southeast) cover different areas of A2151, while field '47' covers the center of A2147. --- Name Other name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec V0 Center velocity km/s DV Width velocity km/s fpb Primary beam attenuation factor --- Area Area used for H I mass determinations number=2 1 pix = 6" pix MHI H I mass obtained from spectra integrals 10+8solMass Mext Maximum total H I mass obtained by extending the area 10+8solMass Mpeak H I mass contained within the central beam area 10+8solMass Mint Mass determined form the integrated flux 10+8solMass Channel map centers Alias Galaxy alias number= Offsets of the fitted peak position from the H I centroid position as given in table2.dat. number= The peak and integrated H I mass contained in the velocity channel similar to the last two columns of table2.dat. --- cz Center velocity of the channel number= Offsets of the fitted peak position from the H I centroid position as given in table2.dat. number= The peak and integrated H I mass contained in the velocity channel similar to the last two columns of table2.dat. km/s oRA Right ascension offset Offsets of the fitted peak position from the H I centroid position as given in table2.dat. number= Offsets of the fitted peak position from the H I centroid position as given in table2.dat. number= The peak and integrated H I mass contained in the velocity channel similar to the last two columns of table2.dat. arcsec oDE Declination offset number= Offsets of the fitted peak position from the H I centroid position as given in table2.dat. number= The peak and integrated H I mass contained in the velocity channel similar to the last two columns of table2.dat. arcsec Mpeak Peak H I mass in the channel The peak and integrated H I mass contained in the velocity channel similar to the last two columns of table2.dat. number= Offsets of the fitted peak position from the H I centroid position as given in table2.dat. number= The peak and integrated H I mass contained in the velocity channel similar to the last two columns of table2.dat. 10+8solMass Mint Integrated H I mass in the channel number= Offsets of the fitted peak position from the H I centroid position as given in table2.dat. number= The peak and integrated H I mass contained in the velocity channel similar to the last two columns of table2.dat. 10+8solMass Patricia Bauer CDS 1998 Feb 04 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 29-Aug-1997 UNKNOWN UNKNOWN table2.dat was prepared via OCR at CDS. J_AJ_113_1939.xml Radio observations of 4079 quasars J/AJ/113/2000 J/AJ/113/2000 New quasar radio detections Radio observations of 4079 quasars O B Bischof R H Becker Astron. J. 113 2000 1997 1997AJ....113.2000B VII/188 : Quasars and Active Galactic Nuclei (7th Ed.) (Veron+ 1996) QSOs Radio sources Using the NVSS radio catalog, we have searched for radio emission from 4079 quasars taken from the 1996 version of the Veron-Cetty & Veron [ESO Scientific Report No.X (1996, Cat. <VII/188>)] quasar catalog. The comparison resulted in the positive detection of radio emission from 799 quasars of these, 168 are new radio detections. Examination of the radio luminosities shows a dramatic increase in 9 the fraction of radio-loud quasars from the current epoch to z=0.5 and a gradual decline beyond z=1.0. Inspection of the radio-loud fraction as a function of MB shows little dependence fainter than M_B_=-29.5.
New quasar radio detections RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec z Redshift --- S1.4GHz Flux density at 1.4GHz mJy BMag Absolute B magnitude mag log(L8.4) Radio luminosity at 8.4GHz [solLum] table1.tex LaTeX version of table1 James Marcout, Patricia Bauer CDS 1997 Oct 10 Otto Bischof <obischof@igpp.llnl.gov> J_AJ_113_2000.xml The I Band Tully-Fisher Relation for Cluster Galaxies: Data Presentation J/AJ/113/22 J/AJ/113/22 Tully-Fisher Relation. I. The I Band Tully-Fisher Relation for Cluster Galaxies: Data Presentation R Giovanelli M P Haynes T Herter N P Vogt G Wegner J J Salzer L N Da Costa W Freudling Astron. J. 113 22 1997 1997AJ....113...22G Clusters, galaxy Morphology Photometry Radial velocities Observational parameters which can be used for redshift-independent distance determination using the Tully-Fisher (TF) technique are given for 782 spiral galaxies in the fields of 24 clusters or groups. I band photometry for the full sample was either obtained by us or compiled from published literature. Rotational velocities are derived either from 21 cm spectra or optical emission line long-slit spectra, and converted to a homogeneous scale. In addition to presenting the data, a discussion of the various sources of error on TF parameters is introduced, and the criteria for the assignment of membership to each cluster are given.
Galaxy parameters, by cluster Cluster Cluster name --- Name1 First identification name If the galaxy is listed in the UGC catalog, the UGC number is listed first; if not, the first listing corresponds to the author's internal coding number. --- Name2 Second identification name The second name is added with the following priority scheme: NGC or IC number; CGCG number in the form "field-number"; for southern galaxies, if and NGC or IC number is not available the ESO/Uppsala catalog name is given. --- RAh Right ascension, 1950.0 h RAm Right ascension, 1950.0 min RAs Right ascension, 1950.0 s DE- Sign of declination --- DEd Declination, 1950.0 deg DEm Declination, 1950.0 arcmin DEs Declination, 1950.0 arcsec T Hubble morphological type Morphological type code in the RC3 scheme, where 1 corresponds to Sa, 3 to Sb, 5 to Sc, etc. If the code is followed by a B, the galaxy disk has an identifiable bar. --- Vcmb Radial velocity in the Cosmic Microwave Background (CMB) reference frame km/s Theta Angular distance from center of cluster deg Mem Membership code c - galaxy is considered a bona fide cluster member g - galaxy is sufficiently removed from the cluster center that cluster membership cannot be safely assigned; the galaxy is, however, in the periphery of the cluster, at roughly the same redshift and it is a nearby supercluster member f - foreground galaxy b - background galaxy --- W Measured velocity width km/s W1 Velocity width, corrected except for inclination km/s Wcor Velocity width, converted to edge-on km/s Inc Adopted inclination of plane of disk deg log(Wcor) Log10 of Wcor --- e_log(Wcor) Estimated uncertainty in log(Wcor) The uncertainty takes into account both measurement errors and uncertainties arising from the corrections. The value (11), for example is equivalent to +/- 0.011. 10-3 Imag Measured and extrapolated I band mag. Measure I band magnitude, extrapolated to infinity assuming that the surface brightness profile of the disk is well described by an exponential function; this value is sometimes adopted as an average of two or more measurements, as footnoted. mag Icor Corrected apparent magnitude Apparent magnitude, to which k-term, galactic, and internal extinction corrections were applied. mag Mcor Corrected absolute magnitude Absolute magnitude, computed assuming that the galaxy is at the distance indicated either by the cluster redshift, if the galaxy is a member, or by the galaxy redshift if not. mag e_Mcor Uncertainty of Mcor The uncertainty on the magnitude is the sum in quadrature of the measurement errors and the estimate of the uncertainty in the corrections applied to the measured parameter. The error estimate does not include the uncertainty on the value of the distance. 0.01mag u_Mcor Uncertainty flag on Mcor --- Ref1 Reference code for photometry A letter code identifies the source for the photometry: a - Authors' photometric observations b - Bernstein et al. 1994AJ....107..1962B, restricted to Coma h - Han & Mould 1992ApJ...396..453H m - Mathewson, Ford, & Buchhorn 1992ApJS...81. 413M p - Pierce & Tully 1988ApJ...330..579P, restricted to Ursa Major s - Bureau et al. 1996ApJ...463...60B, restricted to Fornax x - Combination of different sources as noted --- Ref2 Reference code for velocity width A numerical code identifies the source of velocity width: 0 - Author's 21 cm measurements 1 - Author's optical spectroscopy 2 - Averages of several measurements, see notes 3 - 21 cm observations of Gavazzi 1987ApJ...320...96G and Scodeggio & Gavazzi 1993ApJ...409..110S 4 - 21 cm observations of Bothun et al. 1985ApJS...57..423B, and Aaronson et al. 1989ApJ...338..654A, cross-identified with the compilation of Bottinelli et al. 1990A&AS...82..391B 5 - 21 cm measurements of Mathewson, Ford, & Buchhorn 1992ApJS...81. 413M 6 - Optical spectroscopy of Mathewson, Ford, & Buchhorn 1992ApJS...81. 413M 7 - 21 cm measurements of Pierce & Tully 1988ApJ...330..579P 8 - 21 cm observations of Fontanelli 1984A&A...138...85F; Lewis 1985ApJS...59. 161L; and Schneider et al. 1991ApJS...72.2455S 9 - 21 cm observations of Bureau et al. 1996ApJ...463...60B --- Note Indicates notes in printed paper If an asterisk appears in this column a note for this galaxy is given in the printed paper. --- table2.tex AASTeX version of table2 Patricia Bauer CDS 1997 Feb 11 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 06-Nov-1996 J_AJ_113_22.xml Proton Capture Chains in Globular Cluster Stars. II. Oxygen, Sodium, Magnesium, and Aluminum Abundances in M13 Giants Brighter than the Horizontal Branch J/AJ/113/279 J/AJ/113/279 Proton Capture Chains. II Proton Capture Chains in Globular Cluster Stars. II. Oxygen, Sodium, Magnesium, and Aluminum Abundances in M13 Giants Brighter than the Horizontal Branch R P Kraft C Sneden G H Smith M D Shetrone G E Langer C A Pilachowski Astron. J. 113 279 1997 1997AJ....113..279K J/AJ/112/545 : Proton capture chains in glob. clusters. I. (Pilachowski+ 1996) Abundances Clusters, globular Effective temperatures Stars, giant The tables described here contain equivalent width measurements that were not reported in the printed version of the paper. Observations of 11 giants in the globular cluster M13 fainter than M_V=-1.7 have been obtained with the High Resolution Echelle Spectrograph on the Keck I Telescope. When combined with similar data for brighter giants obtained with the 3.0-m Shane Telescope's Hamilton Echelle spectrograph, these data allow examination of the detailed abundances of oxygen, sodium, magnesium, and aluminium over a wide range of luminosity on the red giant branch. We find that oxygen depletions, correlated with sodium enhancements, can be found in giants with luminosities down to nearly the level of the horizontal branch at M_V=0.3. Aluminum abundances in M13 giants also span a wide range (~1.4dex) and are anticorrelated with the observed magnesium abundances. However, field halo giants of comparable metallicity and evolutionary state exhibit (normal) high abundances of O and Mg and low abundances of Na and Al. Stars in M13 with high sodium and aluminum and low oxygen and magnesium abundances are found at all giant branch luminosities, as are stars with more normal light element abundances (as defined by field halo stars of comparable metallicity). The detailed abundance patterns of the light elements oxygen, sodium, magnesium, and aluminum can be explained most easily as a result of deep mixing and proton capture nucleosynthesis. Evidence in support of this explanation is (a) the constancy of the abundances of Al+Mg and C+N+O, (b) the shift in the distribution of sodium abundances toward higher values and of oxygen abundances toward lower values in cluster giants with surface gravities below log g=1.0. The action of deep mixing, however, is seen not only at the top of the giant branch, but already in some giants even as faint as the level of the horizontal branch. (Copyright) 1996 American Astronomical Society.
M 13 NGC 6205 16 41 41.4 +36 27 37
KeckR45 Equivalent Widths for M13 Stars Lambda Wavelength of identified line 0.1nm ID Line identification --- EP Energy potential eV log(gf) log of oscillator strength --- K228 Equivalent width for M13 star K-228 --- K188 Equivalent width for M13 star K-188 --- K766 Equivalent width for M13 star K-766 --- K168 Equivalent width for M13 star K-168 --- K726 Equivalent width for M13 star K-726 --- K984 Equivalent width for M13 star K-984 --- K955 Equivalent width for M13 star K-955 --- K337 Equivalent width for M13 star K-337 --- K348 Equivalent width for M13 star K-348 --- K1062 Equivalent width for M13 star K-1062 --- K469 Equivalent width for M13 star K-469 --- HamR50 Equivalent Widths for M13 Stars Lambda Wavelength of identified line 0.1nm ID Line identification --- EP Energy potential eV log(gf) log of oscillator strength --- L598 Equivalent width for M13 star L-598 --- L629 Equivalent width for M13 star L-629 --- L194 Equivalent width for M13 star L-194 --- L973 Equivalent width for M13 star L-973 --- L954 Equivalent width for M13 star L-954 --- L835 Equivalent width for M13 star L-835 --- L70 Equivalent width for M13 star L-70 --- tablea.tex AASTeX version of tablea.dat tableb.tex AASTeX version of tableb.dat CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 04-Apr-1997 J_AJ_113_279.xml A New Survey of Stellar Kinematics in the Central Milky Way J/AJ/113/321 J/AJ/113/321 Stellar Kinematics toward A New Survey of Stellar Kinematics in the Central Milky Way G P Tiede D M Terndrup Astron. J. 113 321 1997 1997AJ....113..321T Abundances Photometry Radial velocities Spectroscopy Stars, distances We present the results of a photometric and spectroscopic study of 189 stars in a field at (l,b)=(8.4deg,-6.0deg). We measure radial velocities and selected indices of line strength from the spectra and derive reddening, metallicity, photometric parallaxes, and azimuthal rotation velocities and dispersion. We find an average reddening and extinction to the field of E(V-I)=0.43+/-0.09 and A_V=1.07+/-0.22. We use distances derived from photometric parallaxes and find that the distribution of stars along this line of sight is not strongly peaked at the tangent point. In an attempt to understand the apparent decrease in line-of-sight velocity dispersion with increasing metallicity, we divide our sample into metal-rich and metal-poor groups. Though we lack enough stars to statistically analyze each group, we find the average distances of the metal-rich and metal-poor groups to be, <R>=3.1kpc and <R>=7.0kpc. Excluding stars in our sample which are likely to be in the foreground disk, we calculate a rotational velocity for the bulge of Vrot=97+/-9km/s, {sigma}_phi_=71+/-11km/s. Combining this result with studies at other (l,b), we find a rotation rate for the bulge of 10.6+/-0.6km/s/deg or 77+/-5km/s/kpc. We conclude that when attempting to understand the properties of stars along lines of sight into the bulge it is important to consider the line-of-sight distribution of the stars, especially when more than a few degrees from the galactic center. (Copyright) 1997 American Astronomical Society.
Astrometry, photometry, radial velocity, and distance modulus Star Star number --- RAh Right ascension, epoch B1950 h --- Always ':' --- RAm Right ascension, epoch B1950 min --- Always ':' --- RAs Right ascension, epoch B1950 s DE- Declination sign --- DEd Declination, epoch B1950 deg --- Always ':' --- DEm Declination, epoch B1950 arcmin --- Always ':' --- DEs Declination, epoch B1950 arcsec Vmag V magnitude mag e_Vmag Error in Vmag mag V-I V-I color mag e_V-I Error in V-I mag HRV Heliocentric radial velocity km/s e_HRV Error in HRV km/s DMod Distance modulus, (m-M)_0_ mag e_DMod Error in DMod mag Transformed indices and calculated [Fe/H] Star Star number --- Fe5270 Fe5270 index number=1 Central bandpass Continuum bandpass -------------------------------------------------- Fe 5270 5248.00-5286.75 5235.50-5249.25 5288.00-5319.25 Fe 5335 5314.75-5353.50 5307.25-5317.25 5356.00-5364.75 -------------------------------------------------- mag e_Fe5270 Error in Fe5270 mag Fe5335 Fe5335 index number=1 Central bandpass Continuum bandpass -------------------------------------------------- Fe 5270 5248.00-5286.75 5235.50-5249.25 5288.00-5319.25 Fe 5335 5314.75-5353.50 5307.25-5317.25 5356.00-5364.75 -------------------------------------------------- mag e_Fe5335 Error in Fe5335 mag Hbeta Hbeta index mag e_Hbeta Error in Hbeta mag [Fe/H] Metallicity [Fe/H] [Sun] e_[Fe/H] Error in [Fe/H] [Sun] table1.tex AASTeX version of table1.dat table3.tex AASTeX version of table3.dat CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 04-Apr-1997 J_AJ_113_321.xml U,B,V Light Curves of the Short-Period Solar-Type Eclipsing Binary, V417 Aquilae J/AJ/113/401 J/AJ/113/401 UBV light curves of V417 Aql U,B,V Light Curves of the Short-Period Solar-Type Eclipsing Binary, V417 Aquilae R G Samec B R Pauley B J Carrigan Astron. J. 113 401 1997 1997AJ....113..401S Binaries, eclipsing Photometry, UBV A complete photometric analysis of U,B,V photometry for the short-period solar-type V417 Aquilae is presented. Seven epochs of minimum light were determined from our observations covering two primary and five secondary eclipses. A period study covering some 58,000 orbital cycles reveals two distinct eras of constant period connected by what may be a smooth transition. The periods determined for the two eras are nearly the same, differing by ~0.16s. During the intervening 23 years, a 0.1d jump in residuals takes place. The light curves show that V417 Aql is a W-type W UMa system with a 25min time of constant light in the primary minimum. The light curves are fairly symmetrical. A simultaneous three-color solution was computed using the Wilson synthetic light-curve code. Our photometry in conjunction with the solution reveal that V417 Aql consists of G0 V and F9 V spectral type components in contact with a 19% fill-out and a mass ratio of 0.37. Its nearly equal eclipse depths, the low mass ratio, and the moderate fill-out suggest that V417 Aql may be evolving into an A-type W UMa binary. (Copyright) 1997 American Astronomical Society.
V417 Aql 19 35 24.0 +05 50 19
UBV-band observations of V417 Aql HJD Heliocentric Julian Date d Band Band --- dmag Delta magnitude mag CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 04-Apr-1997 J_AJ_113_401.xml Groups of Galaxies in the Northern CfA Redshift Survey J/AJ/113/483 J/AJ/113/483 Groups of Galaxies Groups of Galaxies in the Northern CfA Redshift Survey M Ramella A Pisani M J Geller Astron. J. 113 483 1997 1997AJ....113..483R VII/193 : ZCat (The CfA Redshift Catalogue) Version June 1995 (Huchra+ 1995) Galaxy catalogs Velocity dispersion We use a friends-of-friends algorithm to identify loose groups from the northern CfA2 survey covering the region 8h<={alpha}_(1950)_<=17h and 8.5{deg}<={delta}_(1950)_<=44.5{deg}. There are 406 groups; 149 of these contains five or more members within the survey. Geometric simulations guide our choice of the selection parameters; {delta}{rho}/{rho}=80 is the limiting density contrast and V0=350km/s is the fiducial velocity linking parameter. The geometric simulations are particularly important for evaluating the impact of large-scale structure (e.g., the Great Wall) on group selection. The physical parameters of this large sample are coincident with our earlier results [126 groups in Ramella et al. (1989ApJ...344..522R)]: the median velocity dispersion in 192 (156; 229)km/s and the median blue log(M/L) is 2.38 (2.20; 2.52). The mass-to-light ratio (M/L) is in units of Msun/Lsun for an assumed Hubble constant, H0=100km/s/Mpc. The numbers in parentheses are 99% confidence limits. This group catalog provides a substantially larger sample for statistical studies than has been previously available. For example, it provides a more substantial sample for estimation of the distribution of group velocity dispersions and of the group-group correlation function. (Copyright) 1997 American Astronomical Society.
List of the values of group parameters for d{rho}/{rho}=80 and V_0_=350km/s ID Identification of group --- Nmemb Number of members --- RAh Mean right ascension 1950 h RAm Mean right ascension 1950 min DE- Sign declination (always blank) --- DEd Mean declination 1950 deg DEm Mean declination 1950 arcmin cz Mean redshift of members km/s e_cz Velocity dispersion km/s log(L) Log of total luminosity [solLum] Rh Virial radius Mpc t(cr) Crossing time (in units of Hubble time) --- log(M) Log of virial mass [solMass] log(M/L) Log of mass-to-light ratio [Sun] table1.tex AASTeX version of table1.dat CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 04-Apr-1997 J_AJ_113_483.xml Globular Cluster Photometry with the Hubble Space Telescope. VI. WF/PC-I Observations of the Stellar Populations in the Core of M13 (NGC 6205) J/AJ/113/669 J/AJ/113/669 Stars in M13 core Globular Cluster Photometry with the Hubble Space Telescope. VI. WF/PC-I Observations of the Stellar Populations in the Core of M13 (NGC 6205) R L Cohen P Guhathakurta B Yanny D P Schneider J N Bahcall Astron. J. 113 669 1997 1997AJ....113..669C J/AJ/107/1745 : HST UVI photometry of M15. II. (Yanny+, 1994) J/AJ/108/1786 : Blue stragglers + variable stars in M3 (Guhathakurta+, 1994) Guhathakurta et al., Paper I. 1992AJ....104.1790G Yanny et al., Paper II. 1994AJ....107.1745Y, cat. <J/AJ/107/1745> Guhathakurta et al., Paper III. 1994AJ....108.1786G, Cat. <J/AJ/108/1786> Guhathakurta et al., Paper V. 1996AJ....111..267G Clusters, globular Photometry We study the dense core of the globular cluster Messier 13 (NGC 6205) using pre-refurbishment Planetary Camera-I images obtained with the Hubble Space Telescope. Short exposures (60s) through the F555W and F785LP filters (similar to Johnson V and I, respectively) have been used to obtain V and I photometry of 2877 stars brighter than V~20 in a 1.25arcmin^2^ region of the cluster including its core and extending out to r~66arcsec (2.3pc) from its center. The sample is complete to V~=18.3 (the main sequence turnoff) and the 1{sigma} photometric error is about 0.1mag. We find 15 blue straggler star candidates and 10 other possible blue stragglers in this region of M13. Their specific frequency is in the range F_(BSS)=0.04-0.07, comparable to what is observed near the centers of other dense clusters. A comparison between M13's observed V band stellar luminosity function and a theoretical model (Bergbusch & Vandenberg, 1992ApJS...81..163B) for the luminosity function of an old, metal-poor cluster shows that the model predicts too few of the brightest red giants (V~12.5-15) by a factor of two relative to subgiants/turnoff stars (>6{sigma} effect). The radial distributions of red giants, blue stragglers, and subgiants are consistent with one another, and are well fit by a King profile of core radius r_(core)_=38+/-6arcsec (90% confidence limits) or 1.3pc. Stars in the blue horizontal branch of M13, however, appear to be centrally depleted relative to other stellar types. We combine data from three dense ``King model clusters,'' M13, M3, and 47 Tuc, and two post core collapse clusters, M30 and M15, and compare the distributions of various stellar types as a function of (r/r_(half light)_) and (r/r_(core)_). The horizontal branch stars in the combined sample appear to be centrally depleted relative to the giants (97% significance), this depletion is only a 1-2{sigma} effect in each of the clusters taken individually. The blue stragglers in the combined sample are centrally concentrated relative to the giants. (Copyright) 1997 American Astronomical Society.
HST
Stars in the core of M13 ID Identification number ---- dRA R.A. J2000 offset from star #5540 All positions are on the equinox J2000 coordinate system, and are measured relative to the reference star U (#5540) whose coordinates are: RA = 16h 41m 41.61s, DE = +36d 27' 42.06", accurate to about 0.25 arcsec. arcsec dDE Dec. J2000 offset from star #5540 arcsec CCD PC number of the CCD --- r Angular distance from center of M13 arcsec F555W F555W magnitude mag F785LP F785LP magnitude mag Vmag V magnitude mag Imag I magnitude mag V-I V-I color mag CDS 1997 Jul 03 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 09-Apr-1997 J_AJ_113_669.xml M-Subdwarfs: Spectroscopic Classification and the Metallicity Scale J/AJ/113/806 J/AJ/113/806 M-Subdwarfs M-Subdwarfs: Spectroscopic Classification and the Metallicity Scale J E Gizis Astron. J. 113 806 1997 1997AJ....113..806G III/198 : PMSU (Palomar/MSU nearby star spectroscopic survey; Hawley+ 1997) Bessell, 1990, Astron. Astrophys. Suppl. 83, 357. (1990A&AS...83..357B) Dawson & Forbes, 1992, Astron. J. 103, 2063. (1992AJ....103.2063D) Dawson & Forbes, 1989, Pub. Astron. Soc. Pac. 101, 614. (1989PASP..101..614D) Doyle and Butler, 1990, Astron. Astrophys. 235, 335. (1990A&A...235..335D) Eggen, 1979, Astrophys. J. Suppl. 39, 89. (1979ApJS...39...89E) Eggen, 1987, Astron. J. 92, 379. (1987AJ.....93..379E) Giclas et al., 1971, Lowell Proper Motion Survey (Flagstaff, AZ: Lowell Obs.). ADC Cat. <1079>. Gliese & Jahreiss, 1991, Preliminary Version of the Third Catalog of Nearby Stars (CNS3), ADC Cat. <5070> Gliese, 1969, Veroff. Astr. Rechen-Instituts, Heidelberg, Nr. 22. Gliese & Jahreiss, 1979, Astron. Astrophys. Suppl., 38, 423. (1979A&AS...38..423G) Gizis, 1997, Astron. J., 113, 806 (1997AJ....113..806G) Harrington & Dahn, 1980, Astron. J. 85, 454. (1980AJ.....85..454H) Leggett, 1992, Astrophys. J. Suppl. 82, 351. (1992ApJS...82..351L) Luyten, 1979, Catalogue of stars with proper motions exceeding 0.5 arcsec annually (Minneapolis: U Minnesota). ADC Cat. <1098> Monet et al., 1992, Astron. J. 103, 638. (1992AJ....103..638M) Reid, 1982, Mon. Not. R. Astron. Soc. 201, 51. (1982MNRAS.201...51R) Reid et al., 1995, Astron. J. 110, 1838. (1995AJ....110.1838R) Ruiz & Anguita, 1993, Astron. J. 105, 614. (1993AJ....105..614R) Ryan, 1992, Astron. J. 104, 1144. (1992AJ....104.1144R) Tinney et al., 1995, Astron. J. 110, 3014. (1995AJ....110.3014T) Van Altena et al., 1991, General Catalog of Trigonometric Stellar Parallaxes: Preliminary Version. (See ADC Cat. <1238>) Weiss, 1984, Astrophys. J. Suppl. 55, 289. (1984ApJS...55..289W) Weiss, 1988, Astron. J. 96, 171. (1988AJ.....96.1710W) Weiss, 1991, Astron. J. 101, 1882. (1991AJ....101.1882W) Weis & Upgren, 1982, Pub. Astron. Soc. Pac. 94, 821. (1982PASP...94..821W) Woolley et al., 1970, R. Obs. Ann., No. 5. ADC Cat. <5032>. Photometry Radial velocities Spectroscopy Stars, M-type Stars, population II Stars, subdwarf We present a spectroscopic classification system for M-dwarfs and M-subdwarfs based on quantitative measures of TiO and CaH features in the region 6200 - 7400 Angstroms. Our sample of cool stars covers the range from solar metallicity stars to the most extreme subdwarfs known. Using synthetic spectra computed by Allard and Hauschildt (1995), we derive metallicities for the stars. Stars are classified as dwarfs (M V), subdwarfs (sdM), or extreme subdwarfs (esdM). These classifications correspond to [m/H] = 0.0, -1.2, and -2.0 respectively. Our metallicity scale agrees with theoretical HR diagrams and HST globular cluster measurements. We discuss some nearby subdwarfs of particular interest in light of our metallicity scale. We include photometry compiled from the literature.
Spectroscopic observations (table 2) LHS Number in LHS catalog Gl - Gliese (1969, Veroff. Astr. Rechen-Instituts, Heidelberg, Nr. 22) GJ - Gliese & Jahreiss =1979A&AS...38..423G Wo - Woolley et al (1970, R. Obs. Ann., No. 5) =Cat. <V/32> LHS - Luyten Half-Second Catalogue =Cat. <I/87> LP - Luyten Palomar proper-motion catalogue G - Giclas et al (1971, Lowell Proper Motion Survey) =Cat. <I/79> Sm - Smethers, see Reid (1982, MNRAS, 201, 51) TVLM - Tinney Very Low Mass, see Tinney et al. (1995AJ....110.3014T) --- Name Other name --- TiO5 TiO5 index: F(7126-7135)/F(7042-7046) --- CaH1 CaH1 index: F(6380-6390)/F (6345-6355,6410-6420)) --- CaH2 CaH2 index: F(6814-6846)/F(7042-7046) --- CaH3 CaH3 index: F(6960-6990)/F(7042-7046) --- RV Radial Velocity Radial velocity for LHS 2715 has been deleted; it was incorrect. km/s Sp Spectral type --- code Telescope code Source of spectroscopic data: 60 - Palomar 60-in. telescope 100 - Las Campanas 100-in. telescope 200 - Hale 200-in. (Palomar) telescope 200a - Hale 200-in. (Palomar) telescope, August 1995 setup RHG - Taken from Reid et al. (1995AJ....110.1838R) --- Photometry (table 4) LHS Number in LHS catalog --- V Apparent V magnitude mag B-V B-V color mag V-R V-R (Cousins) color mag R-I R-I (Cousins) color mag V-I V-I (Cousins) color mag Plx Trigonometric parallax arcsec e_Plx Uncertainty {sigma} of parallax arcsec DeltaLK Lutz-Kelker correction Blank in Lutz-Keller correction indicates a null. -9.99 indicates that the Lutz-Kelker correction is undefined but < -0.80, as symbolized by "L" in the original paper. mag MV Absolute V magnitude Absolute magnitude of LHS 2497 includes 0.75 magnitude correction for unresolved companion mag ref Source of parallax and photometry Dr. Jahreiss has brought to our attention the fact that DF89's photometry of LHS 272 is inconsistent with the results of Doyle and Butler (1990A&A...235..335D), Eggen, and Weis. Our comparison of the spectrum to other subdwarfs suggests that DF89's photometry is too red; thus, we adopt the other photometry for this electronic version. References for the trigonometric parallaxes and photometry are: B - Bessell (1990A&AS...83..357B) CNS3 - Gliese and Jahreiss (1991, ADC Cat. <5070>) DF89 - Dawson and Forbes (1989PASP..101..614D) DF92 - Dawson and Forbes (1992AJ....103.2063D) E79 - Eggen (1979ApJS...39...89E) E87 - Eggen (1987AJ.....93..379E) HD - Harrington and Dahn (1980AJ.....85..454H) L - Leggett (1992ApJS...82..351L) M92 - Monet et al. (1992AJ....103..638M) R - Ryan (1992AJ....104.1144R) RA - Ruiz and Anguita (1993AJ....105..614R) S - SIMBAD T - Tinney et al. (1995AJ....110.3014T) W84 - Weis (1984ApJS...55..289W) W88 - Weis (1988AJ.....96.1710W) W91 - Weis (1991AJ....101.1882W) WU - Weis and Upgren (1982PASP...94..821W) Y - Van Altena et al. (1991) --- John Gizis U.Mass 1997 Dec 15 J_AJ_113_806.xml 21-cm line observations of galaxies in the zone of avoidance. J/AJ/113/905 J/AJ/113/905 HI observations of galaxies 21-cm line observations of galaxies in the zone of avoidance. C A Pantoja D R Altschuler C Giovanardi R Giovanelli Astron. J. 113 905 1997 1997AJ....113..905P J/ApJ/449/527 : Galaxies in the zone of avoidance (Lu+ 1995) J/A+AS/110/269 : Galaxies in the "zone of avoidance". I. (Weinberger+, 1995) J/A+AS/117/1 : Galaxies in the "zone of avoidance". II. (Seeberger+, 1996) J/A+AS/117/369 : Galaxies in the "zone of avoidance". III. (Lercher+, 1996) Galaxies, spectra H I data Morphology We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h<={alpha}<=8h, 0{deg}=<{delta}=<37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.
Sample of observed galaxies from the optical catalog Name Galaxy name --- m_Name Multiplicity index on Name --- RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec POSS POSS E print in which the object was discovered --- a Major axis arcmin b Minor axis arcmin Com Comment regarding the quality and appearance of the image ---- HI Object detected in H I (Y: yes, N: no) --- Sample of galaxies from other catalogs. Name Galaxy name --- RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec MType Morphological type --- a Major axis arcmin --- --- b Minor axis arcmin HI Object detected in H I (Y: yes, N: no) --- H I detected galaxies. Name Galaxy name --- n_Name Note on name number=1 a : At this position lies a bright star, SAO 076738. It is a region with many absorption nebulae (b~-10{deg}) with a diffuse object northeast of this IRAS source. b : This is a galaxy located below the galactic plane at b~-5{deg} in a region with many absorption nebulae. It has a very faint image on the E print (it is not see on the O) and corresponds to the object with the largest H I mass in our sample (M_HI_=5.8x10^10^M_{sun}_). c : Possibly part of an interacting system based on the H I profile and on the neighborhood of other galaxies. d : The negative feature in the profile is probably another galaxy detected in the off scan but no obvious counterpart was found in the POSS prints. e : Pair of galaxies. * : indicates corrections vs the original publication (suggested by H. Andernach) and concerns the sources: 0653+06 (0653+16 in the original publication) +02-18-008 (+02-18-08 in the original publication) 0617+06 (0622+07 in the original publication) These corrections were effectively done on 28-May-1998 --- RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec HVel HI-derived systemic heliocentric velocity km/s e_HVel rms uncertainty on HVel km/s SHI HI line flux Jy.km/s e_SHI rms uncertainty on SHI Jy.km/s W50 Line width measured at 50% of the peak level on each side of the profile km/s e_W50 rms uncertainty on W50 km/s SHIp Peak flux density of the HI feature mJy rms rms noise of the baselined spectrum measured outside the detected feature mJy MHI HI mass 10+10solMass James Marcout, Patricia Bauer CDS 1997 Oct 02 UNKNOWN UNKNOWN * October 1997: Prepared via OCR at CDS. * 28-May-1998: thanks to verifications done by H. Andernach (heinz@astro.ugto.mx) a few typographical errors were corrected; the modifications indicated at the end of the Note (1) above have also been made following H. Andernach's suggestions. J_AJ_113_905.xml Kinematic Profiles of S0 Galaxies J/AJ/113/950 J/AJ/113/950 Kinematic Profiles of S0 Galaxies Kinematic Profiles of S0 Galaxies D Fisher Astron. J. 113 950 1997 1997AJ....113..950F Radial velocities Velocity dispersion Stellar rotation curves, velocity dispersion profiles, and line of sight velocity distributions (LOSVD) as derived from absorption-lines are presented for the major axes of 18 S0 and two elliptical galaxies. Ionized gas rotation curves and dispersions were measured from the [OIII] 5007A emission line in the 9 S0 galaxies displaying this feature. Minor-axis results are given for 14 of the S0 galaxies and one of the ellipticals. A wide range of behaviors are observed in the rotation and velocity dispersion profiles. These variations could be the result of the superposition of stars and gas belonging to the disks and bulges as well as the possible influences of bars, nuclear disks, and warps. Deviations from a Gaussian LOSVD are found along the major axes of all the galaxies in our sample. As parametrised by the Gauss-Hermite series of orthogonal functions, asymmetric deviations are always found in the inner regions of the S0 galaxies such that the prograde wing of the LOSVD is steeper than the retrograde wing. This is similar to the behavior observed in elliptical galaxies. However, at larger radii these asymmetries can change their sign. We find that in 9 of the 18 S0 galaxies a high-speed tail to the LOSVD develops along the major-axis beyond the central regions. In 3 of these 9 objects the LOSVD asymmetries display a second change of sign with radius such that a low-speed tail is again present and persists to our last measured values. No correlations were found between the sizes of the stellar velocity dispersion gradients and either central velocity dispersion, absolute magnitude, disk-to-bulge ratio, Mg2 or Fe line strength gradients. For the objects in our sample with edge-on orientations a comparison between the minor-axis 'bulge' velocity dispersion gradients and those found in elliptical galaxies indicates that the S0 bulges display, on average, logarithmic gradients approximately 4 times steeper than those found in normal luminous ellipticals. A number of galaxies show particularly interesting features. For the LINER S0 galaxy NGC 3998 we find that the velocity dispersion profiles of both the stars and gas rise sharply towards the center reaching nuclear values of sigma~320km/s. Nuclear disks of rapidly rotating gas are found in NGC 4350 and NGC 4762. A nuclear stellar disk is apparent in the edge-on galaxy NGC 4111 and an extended disk of counterrotating gas is observed in the barred S0 NGC 3941.
Stellar radial velocities and velocity dispersions NGC NGC number --- PA Position angle of observations deg Oslit Offset of the slit with respect to the nucleus --- Axis Axis (Major or Minor) --- Radius Radius measure from center of galaxy arcsec RV Radial velocity km/s e_RV Error in RV km/s Sigma Velocity dispersion km/s e_Sigma Error in Sigma km/s Stellar Gauss-Hermite h3 and h4 terms NGC NGC number --- PA Position angle of observations deg Oslit Offset of the slit with respect to the nucleus --- Axis Axis (Major or Minor) --- Radius Radius measure from center of galaxy arcsec h3 Gaussian-Hermite h_3 parameter The velocity distribution is parametrised by the Gauss-Hermite series of orthogonal functions yielding two measures of the deviations of the line profile from a Gaussian: a parameter h_3 which measures asymmetric deviations, and a parameter h_4 measuring symmetric deviations. --- e_h3 Error in h3 --- h4 Gaussian-Hermite h_4 parameter --- e_h4 Error in h4 --- [OIII] 5007A radial velocities & velocity dispersions NGC NGC number --- PA Position angle of observations deg Oslit Offset of the slit with respect to the nucleus --- Axis Axis (Major or Minor) --- Radius Radius measure from center of galaxy arcsec RV Radial velocity km/s e_RV Error in RV km/s Sigma =-99. Velocity dispersion km/s e_Sigma Error in Sigma km/s Patricia Bauer CDS 1997 Feb 11 AAS CD-ROM series, volume 7, 1996 Lee Brotzman [ADS] 12-Nov-1996 J_AJ_113_950.xml Radial velocities of southern stars obtained with the photoelectric scanner CORAVEL. VIII. Observations of 471 giant stars in omega Centauri." J/AJ/114/1087 J/AJ/114/1087 Omega Cen radial velocities Radial velocities of southern stars obtained with the photoelectric scanner CORAVEL. VIII. Observations of 471 giant stars in omega Centauri." M Mayor G Meylan S Udry A Duquennoy J Andersen B Nordstrom Astron. J. 114 1087 1997 1997AJ....114.1087M Clusters, globular Radial velocities This paper presents a catalog of the mean radial velocities of 471 giant stars in the galactic globular cluster Omega Cen, the large majority of which are confirmed as cluster members. The typical uncertainty in the mean velocities is less than 1kms; a variability indicator and notes on chemical peculiarities are provided. In extension of earlier dynamical analyses of Omega Cen, based on part of the data presented here (Meylan & Mayor 1986A&A...166..122M; Meylan 1987A&A...184..144M; Meylan et al. 1995A&A...303..761M), a companion paper (Merritt et al. 1997AJ....114.1074M) rediscusses the subject, based on the full data set and a new theoretical approach, using nonparametric techniques.
omega Cen NGC 5139 13 26 45.8 -47 28 36
Catalog of mean radial velocities for the {omega} Centauri program stars ID Identification number of the stars number=1 1-6999 for the original numbers from Tables I and II by Woolley (1966ROAn....2....1W) (use in SIMBAD: NGC 5139 NNNN) 7xxx indicate stars with the three last digits as in Table III by Woolley (1966ROAn....2....1W) (use in SIMBAD: Cl* NGC 5139 Mar xxx) 8xxx represent new stars following our own numbering (use in SIMBAD: Cl* NGC 5139 MMU xxx) 9xxx are new stars numbered by Freeman (private communication). (use in SIMBAD: NGC 5139 xxx) 8xxx and 9xxx are located in the figure --- Vmag Visual magnitude mag B-V B-V color index mag Rsec Radial distance from the cluster center arcsec PA Position angle, from North to East rad RV Mean radial velocity km/s e_RV rms uncertainty of the mean radial velocity km/s SigRV rms value of the radial velocity distribution km/s o_RV Number of individual observations for the RV determination --- P(chi2) Probability that the observed SigRV is due to observational error only --- Deltat Span in days between the first and last measurements d Rem Remarks number=2 References: 1: Harding, 1962Obs....82..205H 2: Stock & Wroblewski, 1972PDAUC...2...59S 3: Cohen & Bell, 1986ApJ...305..698C 4: Cowley & Crampton, 1985PASP...97..835C 5: Bond, 1975ApJ...202L..47B 6: Lloyd Evans, 1983MNRAS.204..975L 7: Lloyd Evans, 1986SAAOC..10...11L --- table1.tex LaTeX version of table1.dat Patricia Bauer CDS 1997 Nov 14 Stephane Udry <Stephane.Udry@obs.unige.ch> J_AJ_114_1087.xml NSV 09295: A double-mode RR Lyrae variable J/AJ/114/1190 J/AJ/114/1190 NSV 09295: A double-mode RR Lyrae NSV 09295: A double-mode RR Lyrae variable E Garcia-Melendo C M Clement Astron. J. 114 1190 1997 1997AJ....114.1190G Photometry, CCD Stars, variable The table lists the magnitudes of star NSV 09295 relative to the star GSC 1001.0757 which has a photovisual magnitude PAL-V1=13.43+/-0.36 according to the Guide Star Catalogue. The times listed are the Heliocentric Julian Dates at the time of mid-exposure. An analysis of more than 2000 CCD observations of the field RR Lyrae star NSV 09295 shows that the star is a double-mode RR Lyrae (RRd) variable with P_0_=0.46334d and P_1_=0.34423d. This brings the total of known field RRd stars in the Milky Way galaxy to four. These four variables are compared with the RRd stars in galactic globular clusters and with the field RRd stars in the LMC, and in the Draco and Sculptor dwarf galaxies. It appears that all known RRd stars have a metal abundance of less than [Fe/H]=-1.6. (c) 1997 American Astronomical Society.
NSV 09295 GSC 01001-00723 17 37 25.8 +11 22 25 GSC 01001-1265 17 37 32.3 +11 20 26
The observations HJD Heliocentric Julian Date JD DVmag Delta V magnitude (NSV 09295 - GSC 1001.1265) mag CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 31-Oct-1997 J_AJ_114_1190.xml Spectroscopy of edge-on spirals. J/AJ/114/122 J/AJ/114/122 Spectroscopy of edge-on spirals Spectroscopy of edge-on spirals. R Giovanelli E Avera I D Karachentsev Astron. J. 114 122 1997 1997AJ....114..122G VII/162 : Flat Galaxy Catalogue (Karachentsev+ 1993) Radial velocities Radio lines We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.
Detections UGC/AGC UGC/AGC number number=1 3 to 5 digits: UGC number, Cat. <VII/26> 6 digits: AGC number (Arecibo General Catalog) --- FGC FGC (Flat Galaxy Catalog, Cat. <VII/162>) number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec a Blue angular major diameter, as in FGC arcsec --- --- b Blue angular minor diameter, as in FGC arcsec S Uncorrected 21cm H I flux integral Jy.km/s Sc Corrected 21cm H I flux integral Jy.km/s rms Spectrum rms mJy S/N Signal-to-noise ratio --- HVel Heliocentric velocity km/s W50 Velocity width at 50% level, uncorrected km/s W20 Velocity width at 20% level, uncorrected km/s W50c Velocity width at 50% level, corrected for instrumental, relativistic effects km/s e_W50 Error on the velocity width measurement km/s Code Detection and processing codes number=2 Telexcope/spectrometer configuration of the final spectrum code: a: 20MHz total bandwidth over 512 spectral channels o: 10MHz/252 channels g: 10MHz/192 channels, data taken with the 92-meter telescope in the Green Bank b: 10MHz/512 channels, data taken with the 43-meter telescope in the Green Bank n: 6.4MHz/256 channels, data taken with the Nabcay telescope Smoothing code: H: Hanning only B: convolution with 3 channel boxcar followed by Hanning Quality of the profile for TF applications code: G: Good F: Fair M: marginal detection C: confused S: single peak P: completely unfit for TF use Other codes: s: the galaxy is part of the Sc galaxy project of Giovanelli et al. (1997, Scaling laws in extragalactic astronomy, edited by L. da Costa (ESO, Garching), in press) --- Notes individual note detailed in notes.dat file --- Individual notes to table1.dat UGC/AGC UGC/AGC number --- --- --- FGC FGC name --- Ntot Total number of lines of the note --- Nline Running number of the line, [1, Ntot] --- Note Text of the note --- Non Detections FGC FGC (Flat Galaxy Catalog, Cat. <VII/162>) number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec a Blue angular major diameter arcmin b Blue angular minor diameter arcmin UGC UGC name --- table1.tex LaTeX version of table1.dat table2.tex TeX version of table2.dat Patricia Bauer CDS 1997 Sep 24 Riccardo Giovanelli <riccardo@astrosun.tn.cornell.edu> J_AJ_114_122.xml Fornax globular cluster 3: new color-magnitude diagrams for cluster and surrounding field J/AJ/114/1471 J/AJ/114/1471 Fornax Globular 3 Fornax globular cluster 3: new color-magnitude diagrams for cluster and surrounding field E O Smith R R Michael J D Neill Astron. J. 114 1471 1997 1997AJ....114.1471S J/A+A/317/54 : Fornax cluster 1 and 3 photometry (Jorgensen+ 1997) Clusters, globular Photometry, UBV We present new B-V color-magnitude diagrams for Fornax globular cluster 3 and the surrounding field where our data reach one magnitude below the horizontal branch which is at V_HB_=21.28. After subtracting the field stars from the cluster CMD, we found no evidence for an intrinsic width of the red giant branch because the scatter is only slightly wider than the photometric errors. We determine that there is an intrinsic width to the horizontal branch because the scatter is larger than the photometric errors. After comparing our data with earlier photometry, we find 7 possible variable stars, both within and outside the instability strip, out of a total of 74 horizontal branch stars. We calculate the horizontal branch type of cluster 3 to be of intermediate color, -0.110+/-0.104, which when compared to Fornax cluster 1, having similar metallicity, suggests a second-parameter pair. Five carbon star candidates identified by Jorgensen & Jimenez (1997, Cat. <J/A+A/317/54>) are marked in the field-subtracted color-magnitude diagram. (c) 1997 American Astronomical Society.
Cluster 3 in Fornax 02 39.8 -34 16
Fornax cluster 3 photometry ID Identification number --- Xpos X pixel coordinate number=1 North at the top and east to the left. The image is 233" on a side and the center of the cluster in pixels is at the position of (X, Y)=(675, 1214), RA=02h 37m 44s, DE=-34deg 28' 18". 1 pix = 0.43" pix Ypos Y pixel coordinate number=1 North at the top and east to the left. The image is 233" on a side and the center of the cluster in pixels is at the position of (X, Y)=(675, 1214), RA=02h 37m 44s, DE=-34deg 28' 18". 1 pix = 0.43" pix Vmag V magnitude mag e_Vmag V error mag B-V B-V color mag e_B-V B-V error mag table3.tex AASTeX version of table3.dat table3.ps PostScript version CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 04-Nov-1997 J_AJ_114_1471.xml Deep HST V- and I-band observations of two globular clusters in the halo of M31 J/AJ/114/1488 J/AJ/114/1488 Globulars in M31 Deep HST V- and I-band observations of two globular clusters in the halo of M31 S Holland G G Fahlman H B Richer Astron. J. 114 1488 1997 1997AJ....114.1488H Clusters, globular Photometry We present deep (V=~27) V- and I-band stellar photometry of G302 and G312, two globular star clusters in the halo of M31. These data were obtained using the Hubble Space Telescope's Wide Field/Planetary Camera 2. We find iron abundances of [Fe/H]=-1.85+/-0.12 for G302 and [Fe/H]=-0.56+/-0.03 for G312, consistent with spectroscopic measurements. The color-magnitude diagrams for each cluster show no evidence for an intermediate-aged population of stars, or a second parameter effect in the morphology of the horizontal branch. G302 shows no evidence for a color gradient but the inner regions of G312 are bluer than the outer regions. G312 shows no evidence of ellipticity or an extended halo of stars. G302 has a projected ellipticity of {epsilon}=0.195+/-0.012 with the projected major axis oriented towards the center of M31. G302 also shows evidence of an extended asymmetric stellar halo extending to at least twice the fitted Michie-King tidal radius. The amount of mass beyond the tidal radius of G302 is consistent with the stellar escape rates which have been predicted by N-body simulations of globular clusters in the Galactic tidal field. (c) 1997 American Astronomical Society.
HST G302 SKHB 302 Bol 240 00 45 25.2 +41 05 30 G312 SKHB 312 Bol 379 00 45 58.8 +40 42 32
Stellar photometry for G302 and the surrounding fields Stellar photometry for G312 and the surrounding fields CCD CCD the star was observed on --- ID Identification number number=1 Identification numbers are only unique for stars on a given CCD. --- Xpos X pixel coordinate number=2 1 pix = 0.1". pix Ypos Y pixel coordinate number=2 1 pix = 0.1". pix Vmag V-band magnitude mag e_Vmag 1-sigma uncertainty in Vmag mag 2_Vmag Value of the DAOPHOT Chi statistics for Vmag --- Imag I-band magnitude mag e_Imag 1-sigma uncertainty in Imag mag 2_Imag Value of the DAOPHOT Chi statistics for Imag --- Stellar photometry for G302 Stellar Photometry for G312 CCD CCD the star was observed on --- ID Identification number --- Xpos X pixel coordinate number=1 1 pix = 0.1". pix Ypos Y pixel coordinate number=1 1 pix = 0.1". pix Dist Distance of star from cluster center arcsec Vmag V-band magnitude mag e_Vmag 1-sigma uncertainty in Vmag mag 2_Vmag Value of the DAOPHOT Chi statistics for Vmag --- Imag I-band magnitude mag e_Imag 1-sigma uncertainty in Imag mag 2_Imag Value of the DAOPHOT Chi statistics for Imag --- tables.tex AASTeX version of the tables tables.ps PostScript version of the tables CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 04-Nov-1997 J_AJ_114_1488.xml Properties of the Monoceros R2 Stellar Cluster J/AJ/114/198 J/AJ/114/198 The Monoceros R2 Cluster Properties of the Monoceros R2 Stellar Cluster J M Carpenter M R Meyer C Dougados S E Strom L A Hillenbrand Astron. J. 114 198 1997 1997AJ....114..198C Associations, stellar Photometry, infrared We present an extensive study of the stellar population of an embedded cluster in the MonR2 molecular cloud based upon a wide field (~15'x15') J, H, and K band mosaic, deep near-infrared imaging at J, H, K, and nbL' bands of the central cluster region, and spectroscopic observations of 34 stars. By comparing the properties of the MonR2 cluster with other star forming regions, we ultimately hope to learn how the properties and formation of stars of various masses are related to the local physical conditions. The K band star counts indicate that the MonR2 cluster extends over a ~1.1pcx2.1pc area with a FWHM cluster size of ~0.38pc. Within this region the cluster contains ~309 stars brighter than m_K=14.5m and >~475 stars over all magnitudes with a central stellar volume density of ~9000 stars pc^-3^. We have further explored the properties of the cluster by using the spectroscopic and photometric data to construct an extinction-limited sample of 115 stars in the central 0.77pcx0.77pc region of the cluster that is designed to contain all stars with A_V<=11.3m and stellar masses >=0.1M_{sun}_. As a lower limit, 62% of the stars in this sample contain a near-infrared excess at K and/or L band. The K band excess fraction may be as high as 72% if the accretion characteristics of the stars in the MonR2 cluster are similar to stars in Taurus-Auriga. An initial reconnaissance of the stellar mass function suggests that the ratio of high to low mass stars in the extinction-limited sample is consistent with the value expected for a Miller-Scalo IMF. We do not find compelling evidence for mass segregation in the extinction-limited sample for stellar masses <~2M_{sun}_, although the most massive star (~10M_{sun}_) in the cluster appears to be forming near the cluster center. The properties of the MonR2 cluster are similar to other rich young clusters in the solar neighborhood, such as NGC 2024 and the Trapezium. (c) 1997 American Astronomical Society.
Mon R2 NGC 2176 06 07 46.2 -06 23 09
SQIID photometry of MonR2 IRCAM3 photometry of MonR2 [CMD97] Identification number --- RAh Right ascension (1950) h --- Always ':' --- RAm Right ascension (1950) min --- Always ':' --- RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg --- Always ':' --- DEm Declination (1950) arcmin --- Always ':' --- DEs Declination (1950) arcsec Jmag J band magnitude mag e_Jmag 1-sigma uncertainty in Jmag mag Hmag H band magnitude mag e_Hmag 1-sigma uncertainty in Hmag mag Kmag K band magnitude mag e_Kmag 1-sigma uncertainty in Kmag mag nbL' nbL' band magnitude (table2.dat only) The nbL' filter has a peak response at 3.6{mu}m with a full width at half maximum transmission of 0.065{mu}m. mag e_nbL' 1-sigma uncertainty in nbL' mag Notes Additional notes (table2.dat only) Cross identifications are from Beckwith et al. (1976ApJ...208..390B) and Howard et al. (1994ApJ...425..707H). An asterisk in this column indicates an additional note as listed below: 104 -- Stellar ? 122 -- Non-stellar at H; stellar and nebular components at K and nbL' 124 -- Extended at H and K; likely unresolved stars 129 -- Extended at H and K 151 -- Near IRS5; stellar at J and H; non-stellar at K and nbL' 156 -- Non-stellar 172 -- Non-stellar 193 -- Stellar at J? 214 -- Foreground star 233 -- Extended at H and K 235 -- Extended at K 252 -- Stellar? 254 -- Non-stellar at J and H; stellar and nebular components at K; stellar at nbL' 291 -- Saturated at K; photometry very uncertain in all bands 301 -- Non-stellar at J; stellar and nebulous at H; stellar at K and nbL' 315 -- Non-stellar 319 -- Detected at K, but photometry unreliable 364 -- Stellar with local nebulosity at H and K 372 -- Stellar with local nebulosity at JHK 374 -- Extended at all four bands; likely unresolved stars --- tables.tex AASTeX version of the tables CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 26-Sep-1997 J_AJ_114_198.xml Cross identifications in the region of cluster NGC 1502 J/AJ/114/222 J/AJ/114/222 Cross identifications in NGC 1502 Cross identifications in the region of cluster NGC 1502 A J Weitenbeck Astron. J. 114 222 1997 1997AJ....114..222W I/220 : The HST Guide Star Catalog (Lasker+ 1992) Clusters, open Cross identifications In studying this region Purgathofer (1964AnWie..26...37P) [the SIMBAD numbering], Hoag et al.(1961PUSNO..17..343H), and Dombrovskii and Hagen-Thorn (1964TrLen..20...75D) each set up their own numbering system; subsequent authors used one or another of those or variants or combinations. The region covered is 2 degrees in diameter, centered at: (2000) RA 04 04 53.28 dec +62 19 20.7. This is about 15' west of the cluster, the position of HD 25290.
NGC 1502 C 0403+622 04 07.8 +62 20
Cross Identifications near NGC 1502 by GSC number GSC GSC zone (Cat. <I/220>) --- ID Identification number --- mag Magnitude mag RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Name Other name number=1 Designations of the form NGC 1502 NN are from Purgathofer (1964AnWie..26...37P), those of the form HoagNN and DHNN are from Hoag et al. (1961PUSNO..17..343H) and Dombrovskii and Hagen-Thorn (1964TrLen..20...75D). Hoag et al. (1961PUSNO..17..343H) give a table of 26 numbered stars with photoelectric photometry, and a second, longer, unnumbered table of stars with photographic photometry, which includes the stars in the other table. Reiman and Pfau (1987AN....308..111R) numbered the stars in the second table by continuing the numbering from the first table, calling the first star in the second table 27; this system is used here. ---- Name2 Other name number=1 Designations of the form NGC 1502 NN are from Purgathofer (1964AnWie..26...37P), those of the form HoagNN and DHNN are from Hoag et al. (1961PUSNO..17..343H) and Dombrovskii and Hagen-Thorn (1964TrLen..20...75D). Hoag et al. (1961PUSNO..17..343H) give a table of 26 numbered stars with photoelectric photometry, and a second, longer, unnumbered table of stars with photographic photometry, which includes the stars in the other table. Reiman and Pfau (1987AN....308..111R) numbered the stars in the second table by continuing the numbering from the first table, calling the first star in the second table 27; this system is used here. --- Name3 Other name number=1 Designations of the form NGC 1502 NN are from Purgathofer (1964AnWie..26...37P), those of the form HoagNN and DHNN are from Hoag et al. (1961PUSNO..17..343H) and Dombrovskii and Hagen-Thorn (1964TrLen..20...75D). Hoag et al. (1961PUSNO..17..343H) give a table of 26 numbered stars with photoelectric photometry, and a second, longer, unnumbered table of stars with photographic photometry, which includes the stars in the other table. Reiman and Pfau (1987AN....308..111R) numbered the stars in the second table by continuing the numbering from the first table, calling the first star in the second table 27; this system is used here. ---- Name4 Other name number=1 Designations of the form NGC 1502 NN are from Purgathofer (1964AnWie..26...37P), those of the form HoagNN and DHNN are from Hoag et al. (1961PUSNO..17..343H) and Dombrovskii and Hagen-Thorn (1964TrLen..20...75D). Hoag et al. (1961PUSNO..17..343H) give a table of 26 numbered stars with photoelectric photometry, and a second, longer, unnumbered table of stars with photographic photometry, which includes the stars in the other table. Reiman and Pfau (1987AN....308..111R) numbered the stars in the second table by continuing the numbering from the first table, calling the first star in the second table 27; this system is used here. --- Note Note number=2 4067-862 and 4067-873: The 1855 coordinates for BD +61 649 lies almost exactly halfway between these two GSC stars. Additionally, 4067-414 10.8mag, is about 2.6' from the position 4068-347: This is evidently DH97, though DH do not give a BD number. There are no other stars of similar brightness in the vicinity in the GSC or on the Palomar Sky Survey. --- Cross Identifications near NGC 1502 by cluster member number NGC1502 NGC 1502 (1964AnWie..26...37P) identification number number=1 NGC 1502 1 and 2: There is some confusion in the literature over identification of these two similar stars. In SIMBAD the lower HD number HD25638 = 1 is east of HD25639 = 2, and all the other identifications given there are consistent with this. PPM and DH are two of the places with the reverse of SIMBAD. --- m_NGC1502 Multiplicity index on NGC1502 --- Hoag Hoag (1961PUSNO..17..343H) number number=2 These Hoag et al. stars are not in the GSC: 24, 45, 58, 59, 63, 67, 69, 71, 80, 83, 85, 87, 88, 89, 92, 93, 94. --- Tapia Tapia (1991MNRAS.253..649T) number --- DH DH (1964TrLen..20...75D) number --- GSC GSC 4068- (Cat. <I/220>) number --- Patricia Bauer CDS 1997 Nov 18 UNKNOWN UNKNOWN It is a pleasure to thank Anthony J. Weitenbeck <ajw@sal.wisc.edu> who kindly supplied a copy of this table. J_AJ_114_222.xml Seeing tests at four sites in support of the NPOI project J/AJ/114/2822 J/AJ/114/2822 Seeing Tests for NPOI Project Seeing tests at four sites in support of the NPOI project D J Hutter N M Elias II E R Peterson W B Weaver G Weaver D Mozurkewich F J Vrba R S Simon D F Buscher C A Hummel Astron. J. 114 2822 1997 1997AJ....114.2822H Earth This paper reports astronomical seeing measurements made at four sites in the western United States during 1991-92. This study was conducted as part of the site selection process for the Navy Prototype Optical Interferometer. An extensive series of observations were made at Chews Ridge and Anderson Ridge, CA (~36,000 equivalent FWHM seeing estimates). Observations made from Chews Ridge over 49 nights yield an average FWHM seeing value of ~1.1", while those made from Anderson Ridge over 34 nights yield an average FWHM seeing of ~1.4". However, observations made from Anderson Ridge at a location away from any nearby trees indicate that more open sites in that area may enjoy seeing comparable to that measured at Chews Ridge. Simultaneous free-air, ground-level observations at the U.S. Naval Observatory's Flagstaff Station and at Anderson Mesa, both near Flagstaff, AZ, yield similar seeing values to each other (<=0.1" difference).
Seeing measurements Date Observation date "DD/MM/YY" Tel Telescope number=1 a: 'Unit A' seeing monitor b: 'Unit B' seeing monitor v: 1.55 m NOFS telescope --- UTC UTC time of the observation h Gamma Zenith angle of the observation deg Seeing Full-width-at-half-maximum (FWHM) seeing arcsec Patricia Bauer CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 04-Nov-1997 J_AJ_114_2822.xml The MACHO Project LMC Variable Star Inventory. V. Classification and Orbits of 611 Eclipsing Binary Stars J/AJ/114/326 J/AJ/114/326 MACHO Variables V. The MACHO Project LMC Variable Star Inventory. V. Classification and Orbits of 611 Eclipsing Binary Stars C Alcock R A Allsman D Alves T S Axelrod A C Becker D P Bennett K H Cook K C Freeman K Griest C H S Lacy M J Lehner S L Marshall D Minniti B A Peterson M R Pratt P J Quinn A W Rodgers C W Stubbs W Sutherland D L Welch Astron. J. 114 326 1997 1997AJ....114..326A http://wwwmacho.mcmaster.ca/ : MACHO home pageAlcock et al., Paper I. 1995AJ....109.1653A Alcock et al., Paper II. 1996AJ....111.1146A Alcock et al., Paper III. 1997ApJ...482...89A Alcock et al., Paper IV. 1996ApJ...470..583A Binaries, eclipsing Binaries, orbits Magellanic Clouds Photometry As submitted by the author, 637 PostScript figures containing light curves for the LMC eclipsing binary stars in the V and R bands are contained in a single UNIX tape archive (tar) file. The individual files have names of the form 'machohh:mm:ss.s-dd:mm:ss.ps', which do not conform to the CD-ROM ISO 9660 Standard Interchange Level 1, therefore they have been left in the original tar format. The PostScript figures are available on the CD-ROM. We report the characteristics of 611 eclipsing binary stars in the Large Magellanic Cloud found by using the MACHO Project photometry database. The sample is magnitude limited, and extends down the main sequence to about spectral type A0. Many evolved binaries are also included. Each eclipsing binary is classified according to the traditional scheme of the General Catalogue of Variable Stars (EA and EB), and also according to a new decimal classification scheme defined in this paper. The new scheme is sensitive to the two major sources of variance in eclipsing binary star light curves -- the sum of radii, and the surface-brightness ratio, and allow greater precision in characterizing the light curves. Examples of each type of light curve and their variations are given. Sixty-four of the eclipsing binaries have eccentric, rather than circular, orbits. The ephemeris and principal photometric characteristics of each eclipsing binary are listed in a table. Photometric orbits based on the Nelson-Davis-Etzel model have been fitted to all light curves. These data will be useful for planning future observations of these binaries. Plots of all data and fitted orbits and a table of the fitted orbital parameters are available on the AAS CD-ROM series, Vol. 9, 1997. These data are also available at the MACHO home page (http://wwwmacho.mcmaster.ca/). (c) 1997 American Astronomical Society.
SQIID Photometry of MonR2 RAh Right ascension (J2000.0) h --- Always ':' --- RAm Right ascension (J2000.0) min --- Always ':' --- RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg --- Always ':' --- DEm Declination (J2000.0) arcmin --- Always ':' --- DEs Declination (J2000.0) arcsec Comp Indicator of multiple observations --- Type Classification types The type is in the form: XX/NN, where XX is either EA or EB from the General Catalog of Variable Stars and NN is an integer from 1 to 10, inclusive. The numeric classifications are based on the two major sources of variance in the shapes of the eclipsing binary light curves, (1) the sum of the relative radii (r1 + r2), and (2) the surface brightness ratio Js/Jp. Classes 1, 2, and 3 have a surface brightness ratio near unity; classes 4, 5, and 6 have a surface brightness ratio near 0.5; classes 7, 8, and 9 have a surface brightness ratio near 0.18. Classes 1, 4, and 7 have a sum of radii near 0.4; classes 2, 5, and 8 have a sum of radii near 0.7; classes 3, 6, and 9 have a sum of radii near unity. Class 10 is reserved for "Algol-like" systems in which the effects of a secondary component larger than the primary and a large mass ratio are evident in the light curve from the broad and deep "wings" on the eclipses. --- VMax V magnitude at maximum brightness mag VMinI V magnitude at first minimum mag VMinII V magnitude at second minimum mag V-R V-R color mag Epoch Epoch of the primary minimum JD e_Epoch Standard error of the Epoch JD Per Orbital period d DI Primary eclipse duration (phase units) --- o_Vfilt Number of observations in V filter --- SDv Std deviation of residuals from fits (V) mag o_Rfilt Number of observations in R filter --- SDr Std deviation of residuals from fits (R) mag Notes Notes An asterisk, "*", indicates that there are multiple sets of observations of this star. The line of data above or below the asterisk refers to independent observations of the same star. Other notes are entered in full. --- IRCAM3 Photometry of MonR2 RAh Right ascension (J2000.0) h --- Always ':' --- RAm Right ascension (J2000.0) min --- Always ':' --- RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg --- Always ':' --- DEm Declination (J2000.0) arcmin --- Always ':' --- DEs Declination (J2000.0) arcsec Comp Indicator of multiple observations --- Color Color band for the following data --- Js Surface brightness of the secondary (Jp=1) --- e_Js Error in Js --- rp Radius of the primary solRad e_rp Error in rp solRad k Ratio of the radii --- x Limb-darkening coefficient --- i Orbital inclination deg e_i Error in i deg ecosw e*cos{omega} component of eccentricity --- e_ecosw Error in ecosw --- esinw e*sin{omega} component of eccentricity --- e_esinw Error in esinw --- q Assumed mass ratio --- N Number of observations --- SD Standard deviation of the residuals of the fit --- CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 05-Nov-1997 J_AJ_114_326.xml Spectrophotometry of 237 stars in 7 open clusters J/AJ/114/699 J/AJ/114/699 Spectrophotometry in open clusters Spectrophotometry of 237 stars in 7 open clusters L Clampitt D Burstein Astron. J. 114 699 1997 1997AJ....114..699C I/68 : Positions & Proper Motions in alpha Per (Fresneau 1980) I/163 : US Naval Observatory Pleiades Catalog (Van Flandern 1969) J/MNRAS/257/257 : Proper motions in the Hyades (Reid 1992) III/55 : Radial Velocities in Open Clusters (Mermilliod 1979) II/194 : Photometric study of IC 4665 (McCarthy+ 1969) J/AJ/105/1441 : IC 4665 (Prosser 1993) I/203 : NGC 7092 region PM, UBV-phot and SpClass (Platais 1994) J/other/AcASn/32.176 : Stars of Praesepe (Wang+ 1991) Clusters, open Photometry, uvby Spectrophotometry The final calibrated spectral energy distributions (SEDs; relative to 5556{AA}) for all 237 stars are given in Table 4 according to the cluster identification number, the star HD or BD number, and the night(s) of observation. Table 6 lists the observed B-V and uvby data as obtained from SIMBAD, together with the differences (observed minus predicted) between the colors predicted from the authors' spectrophotometry and the observed colors. Spectrophotometry is presented for 237 stars in 7 nearby open clusters: Hyades, Pleiades, Alpha Persei, Praesepe, Coma Berenices, IC 4665, and M39. The observations were taken by Lee McDonald and David Burstein using the Wampler single-channel scanner on the Crossley 0.9m telescope at Lick Observatory from 1973 July through 1974 December. Sixteen bandpasses spanning the spectral range 3500-7780{AA} were observed for each star, with bandwidths 32, 48, or 64{AA}. Data are standardized to the Hayes-Latham system to mutual accuracy of 0.016mag per passband. The accuracy of the spectrophotometry is assessed in three ways on a star-by-star basis. First, comparisons are made with previously published spectrophotometry for 19 stars observed in common. Second, (B-V) colors and uvby colors are compared for 236 stars and 221 stars, respectively. Finally, comparisons are made for 200 main sequence stars to the spectral synthesis models of Kurucz, fixing logg=4.0 and [Fe/H]=0.0, and only varying effective temperature. The accuracy of tests using uvby colors and the Kurucz models are shown to track each other closely, yielding an accuracy estimate (1{sigma}) of 0.01mag for the 13 colors formed from bandpasses longward of the Balmer jump, and 0.02mag for the 3 colors formed from the three bandpasses below the Balmer jump. In contrast, larger scatter is found relative to the previously published spectrophotometry of Bohm-Vitense & Johnson (1977ApJS...35..461B) (16 stars in common) and Gunn & Stryker (1983, Cat. <III/88>) (3 stars). We also show that the scatter in the fits of the spectrophotometric colors and the uvby filter colors is a reasonable way to identify the observations of which specific stars are accurate to 1{sigma}, 2{sigma}, .... As such, the residuals from both the filter color fits and the Kurucz model fits are tabulated for each star where it was possible to make a comparison, so users of these data can choose stars according to the accuracy of the data that is appropriate to their needs. The very good agreement between the models and these data verifies the accuracy of these data, and also verifies the usefulness of the Kurucz models to define spectrophotometry for stars in this temperature range (>5000K). These data define accurate spectrophotometry of bright, open cluster stars that can be used as a secondary flux calibration for CCD-based spectrophotometric surveys. (c) 1997 American Astronomical Society.
Spectral Energy Distributions for 237 open cluster stars ID Star identification number number=1 Number of star according to the following sources: Hyades (Hya): Van Bueren, 1952BAN....11..385V Pleiades (Ple): Hertzsprung, E., 1947AnLei..19a...1H alpha Per (Per): Heckmann, O. et al. 1956AN....283..109H Praesepe (Pra): Klein-Wassink, W. J., 1927PGro...41....1K Coma Berenices (Com): Trumpler, F. J., 1938LicOB..18..167T IC 4665 (IC4): Kopff, 1943AN....274...69K M39 (M39): Ebbinghausen, E. G., 1940ApJ....92..434E --- Night Nights observed number=2 Night of observation + secondary standard star(s) used for night 1 Jul 17/18, 1973 M39 M39 33 2 Aug 14/15, 1973 Pleiades Ple 785 3 Aug 15/16, 1973 M39,alpha Persei Per 605 4 Sep 15/16, 1973 Pleiades Ple 785 5 Sep 16/17, 1973 Hyades Hya 56 6 Sep 17/18, 1973 alpha Persei,Pleiades Ple 785 7 Sep 18/19, 1973 Pleiades Ple 785 8 Sep 20/21, 1973 Hyades Hya 56 9 Oct 12/13, 1973 Hyades Hya 56 10 Oct 13/14, 1973 Hyades Hya 56 11 Mar 8/ 9, 1974 Hyades,Praesepe,Coma B. Hya 56 12 Mar 9/10, 1974 Coma B. Com 60 13 Apr 10/11, 1974 Praesepe Pra 300 14 May 6/ 7, 1974 Coma B. Com 60 15 May 7/ 8, 1974 Praesepe,Coma B.,IC 4665 Pra 300,Com 60 16 Aug 9/10, 1974 IC 4665 IC4 62 17 Dec 29/30, 1974 Hyades,Pleiades,alpha Persei Hya 56 stan If star is used as secondary standard for that cluster --- 3500 3500-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_3500 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 3571 3571-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_3571 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 3636 3636-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_3636 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 4036 4036-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_4036 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 4167 4167-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_4167 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 4255 4255-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_4255 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 4400 4400-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_4400 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 4565 4565-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_4565 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 4785 4785-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_4785 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 5000 5000-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_5000 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 5263 5263-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_5263 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 5840 5840-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_5840 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 6300 6300-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_6300 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 6710 6710-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_6710 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 7100 7100-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_7100 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- 7400 7400-5556 color number=4 Spectrophotometric colors of the cited filter formed with the 5556 filter (15 colors). All colors are expressed in terms of 0.0001 magnitudes (e.g., a value of 1225 is a color of 1.225mag). mmag u_7400 indicates larger error in color number=3 Indicator if error of observation known to be larger than typical error : = error of 0.03-0.06 mag; * = interpolated value from star color and bracketing observations. --- Star-by-star comparison to filter colors and Kurucz models ID Star identification number number=1 Number of star according to the following sources: Hyades (Hya): Van Bueren, 1952BAN....11..385V Pleiades (Ple): Hertzsprung, E., 1947AnLei..19a...1H alpha Per (Per): Heckmann, O. et al. 1956AN....283..109H Praesepe (Pra): Klein-Wassink, W. J., 1927PGro...41....1K Coma Berenices (Com): Trumpler, F. J., 1938LicOB..18..167T IC 4665 (IC4): Kopff, 1943AN....274...69K M39 (M39): Ebbinghausen, E. G., 1940ApJ....92..434E --- HD HD number of star --- RAh Right Ascension 1950 from SIMBAD h --- Always ':' --- RAm Right Ascension 1950 from SIMBAD min --- Always ':' --- RAs Right Ascension 1950 from SIMBAD s DE- Declination sign --- DEd Declination 1950 from SIMBAD deg --- Always ':' --- DEm Declination 1950 from SIMBAD arcmin --- Always ':' --- DEs Declination 1950 from SIMBAD arcsec Sp Spectral type from SIMBAD number=2 Spectral type from SIMBAD. A colon on either spectral class or luminosity class indicates uncertainty. --- Notes Notes for particular stars number=3 Data come from SIMBAD unless a note is given. The note code is: c: these stars are variable according to SIMBAD d: Luminosity class taken from Mendoza, E. E. 1967BOTT....4..149M e: Spectral class taken from Crawford & Barnes 1972AJ.....77..862C f: Luminosity class taken from Crawford & Barnes, 1972AJ.....77..862C --- Vmag Apparent V mag from SIMBAD mag B-V 9.999? Observed B-V color from SIMBAD mag u-b 9.999? Observed u-b color from SIMBAD mag v-y 9.999? Observed v-y color from SIMBAD mag b-y 9.999? Observed b-y color from SIMBAD mag dB-V 9.999? B-V color diff, US-SIMBAD number=4 The residuals from comparing the spectrophotometric colors with B-V, u-b, v-y, b-y colors from SIMBAD. The color transformations are as follows: Color Transformation Slope Z.P. error Johnson B-V Matthews & Sandage 1.072 0.433 0.021 (1963ApJ...138...30M) Stromgren u-b 3500 - (4565+4785)/2 1.005 0.125 0.024 Stromgren b-y (4565+4785)/2 0.934 0.153 0.013 Stromgren v-y (4036+4167)/2 0.891 0.415 0.032 The color transformation for B-V was done using the airmass = 1 bandpass functions for B and V mag as given by Matthews & Sandage mag du-b 9.999? u-b color diff, US-SIMBAD number=4 The residuals from comparing the spectrophotometric colors with B-V, u-b, v-y, b-y colors from SIMBAD. The color transformations are as follows: Color Transformation Slope Z.P. error Johnson B-V Matthews & Sandage 1.072 0.433 0.021 (1963ApJ...138...30M) Stromgren u-b 3500 - (4565+4785)/2 1.005 0.125 0.024 Stromgren b-y (4565+4785)/2 0.934 0.153 0.013 Stromgren v-y (4036+4167)/2 0.891 0.415 0.032 The color transformation for B-V was done using the airmass = 1 bandpass functions for B and V mag as given by Matthews & Sandage mag n_du-b Bad u-b color comparision number=5 If indicated by a colon (:), this color comparison was not used in determining the color transformations. --- dv-y 9.999? v-y color diff, US-SIMBAD number=4 The residuals from comparing the spectrophotometric colors with B-V, u-b, v-y, b-y colors from SIMBAD. The color transformations are as follows: Color Transformation Slope Z.P. error Johnson B-V Matthews & Sandage 1.072 0.433 0.021 (1963ApJ...138...30M) Stromgren u-b 3500 - (4565+4785)/2 1.005 0.125 0.024 Stromgren b-y (4565+4785)/2 0.934 0.153 0.013 Stromgren v-y (4036+4167)/2 0.891 0.415 0.032 The color transformation for B-V was done using the airmass = 1 bandpass functions for B and V mag as given by Matthews & Sandage mag n_dv-y Bad v-y color comparision number=5 If indicated by a colon (:), this color comparison was not used in determining the color transformations. --- db-y 9.999? b-y color diff, US-SIMBAD number=4 The residuals from comparing the spectrophotometric colors with B-V, u-b, v-y, b-y colors from SIMBAD. The color transformations are as follows: Color Transformation Slope Z.P. error Johnson B-V Matthews & Sandage 1.072 0.433 0.021 (1963ApJ...138...30M) Stromgren u-b 3500 - (4565+4785)/2 1.005 0.125 0.024 Stromgren b-y (4565+4785)/2 0.934 0.153 0.013 Stromgren v-y (4036+4167)/2 0.891 0.415 0.032 The color transformation for B-V was done using the airmass = 1 bandpass functions for B and V mag as given by Matthews & Sandage mag n_db-y Bad b-y color comparision number=5 If indicated by a colon (:), this color comparison was not used in determining the color transformations. --- dkurbl 9.999? Kurucz comparison, blue col number=6 These are the average residuals from the best fit of Kurucz main sequence model spectral energy distributions to the main sequence stars in our sample. dkurbl are the residuals for the three colors with one passband falling below 4000 angstroms. dkurrd are the residuals for the 12 colors with both passbands falling at or above 4000 angstroms. Note that the residuals from the Kurucz fit (dkurbl and dkurrd) are well-correlated with the residuals from the uvby fits (dkurbl with du-b; dkurrd with db-y), so that the size of the color residuals is a good indication of the error of spectrophotometric observation, as detailed in the paper. mag dkurrd 9.999? Kurucz comparison, red col number=6 These are the average residuals from the best fit of Kurucz main sequence model spectral energy distributions to the main sequence stars in our sample. dkurbl are the residuals for the three colors with one passband falling below 4000 angstroms. dkurrd are the residuals for the 12 colors with both passbands falling at or above 4000 angstroms. Note that the residuals from the Kurucz fit (dkurbl and dkurrd) are well-correlated with the residuals from the uvby fits (dkurbl with du-b; dkurrd with db-y), so that the size of the color residuals is a good indication of the error of spectrophotometric observation, as detailed in the paper. mag Vabs Absolute V mag number=7 The absolute V magnitude, extinction corrected, according to the following values for reddening and distances: dist(pc) E(B-V) Praesepe 180 0.03 Hyades 43 0.00 Coma Berenices 90 0.00 M39 290 0.06 Pleiades 180 0.06 IC 4665 470 0.17 alpha Persei 230 0.10 The distances are estimated by a direct fit of the ZAMS line from Mihalas & Binney (1981, Galactic Astronomy (Freeman, New York) p. 106) to the V vs. B-V diagrams as published in our paper. The reddenings come from the 5th edition of the Lund-Strasbourg Catalog (Lynga 1987, Cat. <VII/92>) mag CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997ASU] Oct-01-1997 J_AJ_114_699.xml Systematic errors in the FK5 catalog as determined from CCD observations in the extragalactic reference frame J/AJ/114/850 J/AJ/114/850 Errors in the FK5 Catalog Systematic errors in the FK5 catalog as determined from CCD observations in the extragalactic reference frame R C Stone Astron. J. 114 850 1997 1997AJ....114..850S I/149A : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) - Extension (Fricke+ 1991) Fundamental catalog Positional data This paper presents new positions for 689 FK5 stars determined directly in the extragalactic reference system from CCD scan observations made with the Flagstaff Astrometric Scanning Transit Telescope (FASTT). All the observations were made in 1994-1996 with an accuracy of ~+/-40mas in each coordinate. When these positions are compared with their counterparts in the FK5 catalog, systematic errors in the FK5 are found that vary in both right ascension and declination and can be as large as 100 mas in magnitude. No magnitude-dependent errors in the FK5 were found. Moreover, the true error in FK5 star positions is determined to be ~+/-80mas in both coordinates or two times the expected catalog positional errors. There is an excellent agreement between the systematic errors in the FK5 found in this paper and those presented in Lindegren et al. (1995A&A...304...44L) comparing FK5 and Hipparcos 30-month star positions. By comparing corresponding FASTT and FK5 star positions, the link between the optical and extragalactic reference frames was determined and is given by the following rotations ({omega}_x_,{omega}_y_,{omega}_z_) = (3+/-5, 25+/-5, 16+/-4) (s.e.) mas, which agree well with previous determinations made by other investigators. Two of the rotations ({omega}_y_,{omega}_z_) are significantly larger than their standard errors and, therefore, presumably real. Finally, since these rotations are small (<=25mas), the FK5 and extragalactic reference frames must be closely aligned to one another.
FK5 star positions determined in the extragalactic reference frame with the FASTT CCD meridian telescope Seq Running number --- FK5 FK5 star number (Cat. <I/149>, <I/175>) --- HD HD designation --- Vmag V magnitude taken from FK5 catalog mag RAh Right ascension, J2000 h RAm Right ascension, J2000 min RAs Right ascension, J2000 s e_RAs Standard error in RA 10-4s o_RAh Number of times observed in RA --- EpRA-1900 Mean epoch of RA coordinate (+ 1900) yr pmRA Proper motion in RA taken from FK5 10-2s/yr DE- Declination sign --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec e_DEs Standard error in DE mas o_DEd Number of times observed in DE --- EpDE-1900 Mean epoch of DE coordinate (+ 1900) yr pmDE Proper motion in DE taken from FK5 10mas/yr CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 27-Sep-1997 J_AJ_114_850.xml Direct distances to nearby galaxies using detached eclipsing binaries and Cepheids. I. Variables in the field M31B J/AJ/115/1016 J/AJ/115/1016 M 31B eclipsing binaries and Cepheids Direct distances to nearby galaxies using detached eclipsing binaries and Cepheids. I. Variables in the field M31B J Kaluzny K Z Stanek M Krockenberger D D Sasselov J L Tonry M Mateo Astron. J. 115 1016 1998 1998AJ....115.1016K J/A+AS/126/401 : M 31 Cepheids periods (Magnier+ 1997) http://cfa-www.harvard.edu/~kstanek/DIRECT : Direct Project Binaries, eclipsing Photometry Stars, variable binaries: eclipsing Cepheids galaxies: distances and redshifts galaxies: individual (M 31) Local Group We have undertaken a long-term project, DIRECT, to obtain the direct distances to two important galaxies in the cosmological distance ladder - M31 and M33 - using detached eclipsing binaries (DEBs) and Cepheids. While rare and difficult to detect, DEBs provide us with the potential to determine these distances with an accuracy better than 5%. The extensive photometry obtained in order to detect DEBs provides us with good light curves for the Cepheid variables. These are essential to the parallel project to derive direct Baade-Wesselink distances to Cepheids in M31 and M33. For both Cepheids and eclipsing binaries, the distance estimates will be free of any intermediate steps. As a first step in the DIRECT project, between 1996 September and 1997 January we obtained 36 full nights on the Michigan-Dartmouth-MIT Observatory 1.3m telescope and 45 full/partial nights on the F.L. Whipple Observatory 1.2m telescope to search for DEBs and new Cepheids in the M31 and M33 galaxies. In this paper, first in a series, we present the catalog of variable stars, most of them newly detected, found in the field M31B [({alpha},{delta})=(11.20{deg}, 41.59{deg}), J2000.0]. We have found 85 variable stars: 12 eclipsing binaries, 38 Cepheids, and 35 other periodic, possible long-period or nonperiodic variables. The catalog of variables, as well as their photometry and finding charts, is available via anonymous ftp and the World Wide Web: http://cfa-www.harvard.edu/~kstanek/DIRECT.
Direct miscellaneous variables in M31B D31B Variable name (DIRECT VNNNN D31B in Simbad) --- RAdeg Right ascension (J2000.0) deg DEdeg Declination (J2000.0) deg Js Variability index J_S_ --- Per Period d Vmax Maximun V magnitude of the system outside eclipse mag Imax Maximun I magnitude of the system outside eclipse mag Rad1 Radius of the binary first component number=1 The radius are in units of the orbital separation --- Rad2 Radius of the binary second component number=1 The radius are in units of the orbital separation --- i Inclination angle of the binary orbit to the line of sight deg e Eccentricity of the orbit --- Com Comments number=2 Ma97 NNN, NNN identification number assigned by Magnier et al., 1997, Cat. <J/A+AS/126/401> --- Direct Cepheids in M31B D31B Variable name (DIRECT VNNNN D31B in Simbad) --- RAdeg Right ascension (J2000.0) deg DEdeg Declination (J2000.0) deg Js Variability index J_S_ --- Per Period d <Vmag> Flux-weighted mean V magnitude mag <Imag> Flux-weighted mean I magnitude mag A Amplitude of the variation --- Com Comments number=1 Ma97 NNN, NNN identification number assigned by Magnier et al., 1997, Cat. <J/A+AS/126/401> --- Direct other periodic variables in M31B Direct miscellaneous variables in M31B D31B Variable name (DIRECT VNNNN D31B in Simbad) --- RAdeg Right ascension (J2000.0) deg DEdeg Declination (J2000.0) deg Js Variability index J_S_ --- Per Period (only in table3.dat) d <Vmag> Error-weighted mean V magnitude mag <Imag> Error-weighted mean I magnitude mag e_<Vmag> rms uncertainty on <Vmag> mag e_<Imag> rms uncertainty on <Imag> mag Com Comments --- Light curves of eclipsing binaries in M31B Light curves of Cepheids in M31B Light curves of other periodic variables in M31B Light curves of miscellaneous variables in M31B D31B Variable name (DIRECT VNNNN D31B in Simbad) --- Band Band --- HJD Heliocentric Julian date d mag Magnitude mag e_mag rms uncertainty on mag mag James Marcout CDS 1998 Apr 06 UNKNOWN UNKNOWN From the Astronomical Journal electronic version J_AJ_115_1016.xml The deep X-ray radio blazar survey. I. Methods and first results. J/AJ/115/1253 J/AJ/115/1253 Deep X-Ray Radio Blazar Survey The deep X-ray radio blazar survey. I. Methods and first results. E S Perlman P Padovani P Giommi R Sambruna L R Jones A Tzioumis J Reynolds Astron. J. 115 1253 1998 1998AJ....115.1253P IX/12 : The WGACAT version of ROSAT sources (White+ 1995) VIII/38 : The Parkes-MIT-NRAO 4.85GHz (PMN) Surveys (Griffith+ 1993-1996) VIII/40 : GB6 catalog of radio sources at 4.85GHz (Gregory+ 1996) VIII/15 : Parkes Radio Sources Catalogue (PKSCAT90) (Wright+ 1990) BL Lac objects QSOs Radio sources Surveys X-ray sources BL Lacertae objects: general quasars: general radio continuum surveys We have undertaken a survey, the Deep X-Ray Radio Blazar Survey (DXRBS), of archived, pointed ROSAT Position Sensitive Proportional Counter data for blazars by correlating the ROSAT WGACAT database with several publicly available radio catalogs, restricting our candidate list to serendipitous flat radio spectrum sources ({alpha}_r_<=0.70, where S_{nu}_{prop}{nu}^-{alpha}_r_^). We discuss our survey methods, identification procedure, and first results. Our survey is found to be 95% efficient at finding flat-spectrum radio-loud quasars (FSRQs; 59 of our first 85 identifications) and BL Lacertae objects (22 of our first 85 identifications), a figure that is comparable to or greater than that achieved by other radio and X-ray survey techniques. The identifications presented here show that all previous samples of blazars (even when taken together) did not representatively survey the blazar population, missing critical regions of (LX, LR) parameter space within which large fractions of the blazar population lie. Particularly important is the identification of a large population of FSRQs (>=25% of DXRBS FSRQs) with ratios of X-ray to radio luminosity >=10^-6^({alpha}_rx_<=0.78). In addition, as a result of our greater sensitivity, the DXRBS has already more than doubled the number of FSRQs in complete samples with 5GHz (radio) luminosities between 10^31.5^ and 10^33.5^ergs/s/Hz, and fills in the region of parameter space between X-ray-selected and radio-selected samples of BL Lac objects. The DXRBS is the very first sample to contain statistically significant numbers of blazars at low luminosities, approaching what should be the lower end of the FSRQ luminosity function.
ROSAT
Positional information 1WGA WGACAT name --- RAh WGACAT right ascension (J2000) h RAm WGACAT right ascension (J2000) min RAs WGACAT right ascension (J2000) s DE- WGACAT declination sign --- DEd WGACAT declination (J2000) deg DEm WGACAT declination (J2000) arcmin DEs WGACAT declination (J2000) arcsec oWGA Offset from field center in X-ray arcsec eWGA WGACAT error number=1 WGACAT positional error circles. This was done as follows: WGACAT was cross-correlated with the Hipparcos Input Catalogue (Cat. <I/196>), and the offsets between the two databases were obtained for six bins of the distance from the WGACAT field center (0'-10', 10'-20', etc.). These values range from 13" (for the inner 10' of the PSPC field) to 53" (for the 50'-60' ring). arcsec RA1h PMN or GB6 right ascension (J2000) h RA1m PMN or GB6 right ascension (J2000) min RA1s PMN or GB6 right ascension (J2000) s DE1- PMN or GB6 declination sign --- DE1d PMN or GB6 declination (J2000) deg DE1m PMN or GB6 declination (J2000) arcmin DE1s PMN or GB6 declination (J2000) arcsec RA2h Optical Counterpart right ascension (J2000) h RA2m Optical Counterpart right ascension (J2000) min RA2s Optical Counterpart right ascension (J2000) s DE2- Optical Counterpart declination sign --- DE2d Optical Counterpart declination (J2000) deg DE2m Optical Counterpart declination (J2000) arcmin DE2s Optical Counterpart declination (J2000) arcsec Source Source number=2 Source codes are: APM: APM survey GB6: Green Bank 6cm catalog, Cat. <VIII/40> PMN: Parkes-MIT-NRAO catalog, Cat. <VIII/27> ATCA: Austalian Telescope Compact Array, this paper NVSS: NRAO VLA Sky Survey, Condon et al., 1998AJ....115.1693C FIRST: FIRST project, Gregg et al., 1996AJ....112..407G; Laurent-Muehleisen et al., 1998, in prep. (see <VIII/51>) --- Offset Absolute offset (X-O) value arcsec eCount Counterpart error arcsec Error Cumulative error arcsec Offset/Error Ratio of Offset to Error --- Newly identified objects 1WGA WGACAT name --- Crate ROSAT count rate ct/s F(0.1-2.0) 0.1-2.0keV flux mW/m2 F1keV Flux density at 1keV uJy log(FX/FR) X-flux to radio-flux ratio --- F6cm Flux density at 6cm mJy SI Radio spectral index --- l_Bmag Limit flag on Bmag --- Bmag B magnitude mag l_Rmag Limit flag on Rmag --- Rmag R magnitude mag Class Classification number=1 Classification is: RG: radio galaxy FSRQ: flat-spectrum radio-loud quasar SSRQ: steep-spectrum radio-loud quasar BL Lac: BL Lac object --- z Redsifht --- u_z Uncertainty flag on z --- Cat Other catalogs number=2 Other catalogs are numbered: 1: RASS Bright Source Catalog, Cat. <IX/10> 2: HBQS, Homogeneous Bright QSO Survey, Cat. <J/A+AS/112/347> 3: V Zwicky Catalog of Galaxies, Cat. <VII/190> 4: 4C, Fourth Cambridge Survey, Cat. <VIII/4> 5: Einstein Slew Survey, Elvis et al., 1992ApJS...80..257E 6: FIRST Bright Quasar Survey, See Cat. <VIII/51> 7: B3, Third Bologna Survey, Cat. <VIII/37> 8: Las Campanas Redshift Survey, Cat. <VII/203> --- Previously identified blazars Name Source name --- Crate ROSAT count rate ct/s F(0.1-2.0) 0.1-2.0keV flux mW/m2 F1keV Flux density at 1keV uJy log(FX/FR) X-flux to radio-flux ratio --- F6cm Flux density at 6cm mJy SI Radio spectral index --- Vmag V magnitude mag Class Classification number=1 Classification is: RG: radio galaxy FSRQ: flat-spectrum radio-loud quasar BL Lac: BL Lac object --- l_z Limit flag on z --- z Redsifht --- u_z Uncertainty flag on z --- Individual notes 1WGA WGACAT name (repeated of more than 1 line) --- Note Text of the note --- Patricia Bauer CDS 1998 Aug 11 UNKNOWN UNKNOWN From AJ electronic version J_AJ_115_1253.xml VRI CCD photometry of supergiant stars in the barred galaxies NGC 925 and NGC 1637 J/AJ/115/130 J/AJ/115/130 NGC 925 & NGC 1637 supergiants VRI CCD photometry VRI CCD photometry of supergiant stars in the barred galaxies NGC 925 and NGC 1637 Y -J Sohn T J Davidge Astron. J. 115 130 1998 1998AJ....115..130S J/AJ/112/2559 : Supergiants in NGC 672 (Sohn+ 1996) J/AJ/109/517 : Photoelectric types of bright galaxies (Buta+ 1995) Sohn & Davidge Paper I. 1996AJ....111.2280S Sohn & Davidge Paper II. 1996AJ....112.2559S, Cat. <J/AJ/112/2559> Photometry, CCD Photometry, VRI Stars, supergiant galaxies: individual (NGC 925, NGC 1637) galaxies: stellar content V, R, and I CCD images obtained with the Canada-France-Hawaii Telescope are used to investigate the bright stellar content of the barred spiral galaxies NGC 925 and NGC 1637. Not counting objects located in H II regions, we detect 295 supergiants in NGC 925 and 266 in NGC 1637. Comparisons with theoretical isochrones indicate that massive star formation in NGC 925 has been ongoing for at least a few tens of millions of years. Most of the supergiants in NGC 925 are younger than 20Myr and have masses between 10 and 60M_{sun}_. The majority of supergiants in NGC 1637 appear to be younger than 40Myr and have initial masses between 8 and 60 M_{sun}_. The luminosity functions of supergiants in both galaxies follow power laws with exponents d(logn)/d(logV)=0.50+/-0.05 for NGC 925 and 0.62+/-0.04 for NGC 1637. These values are shallower than what is seen in most spiral galaxies, although there are some exceptions. Archival Hubble Space Telescope images of NGC 925 are used to assess the effects of blending on our photometric measurements. We conclude that crowding could cause a flattening of the luminosity function and bias the brightnesses of the most luminous stars. The brightest red supergiants are used to estimate the distance moduli of these galaxies. After applying corrections for blending, we find that {mu}_0_=29.67 for NGC 925 and {mu}_0_=29.47 for NGC 1637, corresponding to linear distances of 8.6^+1.1^_-1.0_ and 7.8^+1.0^_-0.9_Mpc, respectively. The distance computed for NGC 925 is in good agreement with that recently derived from Cepheids.
NGC 925 02 27 16.5 +33 34 14 NGC 1637 04 41 28.1 -02 51 53
Positions, magnitudes and colors of NGC 925 stars Positions, magnitudes and colors of NGC 1637 stars [SD98] Identification number number=1 In Simbad, [SD98] NGC 925 NNN for table3.dat [SD98] NGC 1637 NNN for table4.dat --- Xc X coordinate number=2 The field centers are 2h 24m 16.5s +33deg 20' 48" (1950) for NGC 925 4h 38m 57.6s -02deg 57' 35" (1950) for NGC 1637 1 pix = 1.13". pix Yc Y coordinate number=2 The field centers are 2h 24m 16.5s +33deg 20' 48" (1950) for NGC 925 4h 38m 57.6s -02deg 57' 35" (1950) for NGC 1637 1 pix = 1.13". pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag V-I V-I colour index mag e_V-I rms uncertainty on V-I mag R-I R-I colour index mag e_R-I rms uncertainty on R-I mag HK1 HII region identification number=3 Hodge & Kennicutt (1983AJ.....88..296H) HII region identification <HK NGC 925 NNN> in Simbad. Only in table3.dat --- --- Dash --- HK2 HII region identification number=3 Hodge & Kennicutt (1983AJ.....88..296H) HII region identification <HK NGC 925 NNN> in Simbad. Only in table3.dat --- Patricia Bauer CDS 1998 Mar 09 UNKNOWN UNKNOWN Copied from the electronic version of AJ J_AJ_115_130.xml Early evolution of the Galactic halo revealed from Hipparcos observations of metal-poor stars J/AJ/115/168 J/AJ/115/168 Kinematics of red giant and RR Lyrae stars Early evolution of the Galactic halo revealed from Hipparcos observations of metal-poor stars M Chiba Y Yoshii Astron. J. 115 168 1998 1998AJ....115..168C I/196 : Hipparcos Input Catalogue, Version 2 (Turon+ 1993) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Proper motions Stars, giant Stars, variable Galaxy: abundances Galaxy: evolution Galaxy: halo The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]<=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]<=-1.6, is characterized by a lack of systemic rotation [(<U>, <V>, <W>)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(<U>, <V>, <W>)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e<0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]<=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6<[Fe/H]<=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|<1kpc. This disk component appears to constitute only 10% for -1.6<[Fe/H]<=-1 and 20% for -1.4<[Fe/H]<=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.
Hipparcos
Program stars Type Type of the stars RG: Red giants; RR: RR Lyrae --- HIC(P) HIC or HIP (Cat. <I/239>) number --- Name Other name --- plx Trigonometric parallax mas e_plx rms uncertainty on plx mas pmRA* Proper motion in RA time cos{delta} mas/yr e_pmRA* rms uncertainty on pmRA mas/yr pmDE Proper motion in DE mas/yr e_pmDE rms uncertainty on pmDE mas/yr Dist Photometric distance kpc e_Dist rms uncertainty on Dist kpc [Fe/H] Metallicity [Sun] e_[Fe/H] rms uncertainty on [Fe/H] [Sun] RV Radial velocity km/s e_RV rms uncertainty on RV km/s pmRAold Old proper motion in RA arcsec/yr pmDEold Old proper motion in DE arcsec/yr r_Dist References for Dist and [Fe/H] number=1 1: Anthony-Twarog & Twarog, 1994AJ....107.1577A, Cat. <J/AJ/107/1577> 1s: Spectroscopic abundances compiled by Anthony-Twarog & Twarog, 1994 2: Bond, 1980ApJS...44..517B 2s: Spectroscopic abundances compiled by Anthony-Twarog & Twarog, 1994 3: Layden, 1994AJ....108.1016L, Cat. <J/AJ/108/1016> 4: Layden et al., 1996AJ....112.2110L --- --- --- r_RV References for RV number=2 1: Bond 1980ApJS...44..517B 2: Carney & Latham, 1986AJ.....92...60C 3: Norris, Bessell & Pickles, 1985 4: Barbier-Brossat, 1989A&AS...80...67B, Cat. <III/161> 5: Wilson, 1953, Cat. <III/21> 6: Evans, 1978BICDS..15..121J, Cat. <III/42> 7: Griffin et al., 1982MNRAS.198..637G 8: Papers quoted by Bond, 1980ApJS...44..517B 9: Layden, 1994AJ....108.1016L, Cat. <J/AJ/108/1016> --- --- --- r_pmRA* References for proper motions number=3 1: Lick Northern Proper Motion Catalogue, Cat. <I/199> 2: Hipparcos Input Catalogue, Cat. <I/196> 3: Wan, Mao & Ji, 1980, Ann. Shanghai Obs., 2, 1 --- Patricia Bauer CDS 1998 Mar 10 UNKNOWN UNKNOWN Copied from the electronic version of AJ J_AJ_115_168.xml M87, globular clusters, and galactic winds: issues in giant galaxy formation. J/AJ/115/1801 J/AJ/115/1801 VRI photometry of M87 globular clusters M87, globular clusters, and galactic winds: issues in giant galaxy formation. W E Harris G L H Harris D E McLaughlin Astron. J. 115 1801 1998 1998AJ....115.1801H J/ApJS/73/671 : M87 globular clusters BVI photometry (Couture+, 1990) J/AJ/106/493 : Globular clusters in M87 (Lee+, 1993) Clusters, globular Photometry, UBVRI galaxies: elliptical and lenticular, cD galaxies: evolution galaxies: star clusters We have used the high-resolution camera at the Canada-France-Hawaii Telescope to obtain VRI photometry of the globular clusters in the innermost 140 of the M87 halo. The results are used to discuss several issues concerning the formation and evolution of globular cluster systems in supergiant elliptical galaxies like M87. Our principal results are as follows: (1) From our deep R-band photometry of the cluster population, we find no significant change in the globular cluster luminosity function (GCLF) with galactocentric radius, for cluster masses M>=10^5^M_{sun}_. This result places constraints on current theoretical predictions of the rate of cluster evolution by tidal shocking and evaporation, indicating that the main effects of dynamical evolution may be felt only on lower mass clusters (<~10^5^M_{sun}_) that are below the faint limit of most current observations. (2) Combining our V-I color indices with other data in the literature, we derive the metallicity gradient and mean metallicity of the clusters from r=9" out to r~500" (~0.7-35kpc). Within the core radius r_c_=1' of the globular cluster system, the metallicity distribution is uniform, but at larger radii the mean metallicity declines steadily as Z/Z_{sun}_~r^-0.9^. (3) The various options for explaining the existence of high specific frequency galaxies like M87 are evaluated. (4) We offer a new explanation for the large observed S_N_ range among the brightest cluster elliptical galaxies (BCGs). It is suggested that these central supergiant E galaxies formed in an exceptionally turbulent or high-density environment which favored a very rapid initial star formation burst. From a total sample of 30 BCGs, we derive empirical scaling relations that relate to this hypothesis. Our analysis favors the view that BCGs began forming at redshifts z>~5, distinctly earlier than most other galaxies.
M 87 NGC 4486 12 30 49.4 +12 23 28
Photometry of brightest clusters Rmag R magnitude mag Xpos X position number=1 Fiducial directions are marked on the borders of Fig.2, with the galaxy center at (0,0). arcsec Ypos Y position number=1 Fiducial directions are marked on the borders of Fig.2, with the galaxy center at (0,0). arcsec V-R V-R colour index mag R-I R-I colour index mag James Marcout, Patricia Bauer CDS 1998 Aug 12 UNKNOWN UNKNOWN From AJ electronic version J_AJ_115_1801.xml The star formation history of the Carina dwarf galaxy. J/AJ/115/1840 J/AJ/115/1840 BV photometry in Carina dwarf galaxy The star formation history of the Carina dwarf galaxy. D Hurley-Keller M Mateo J Nemec Astron. J. 115 1840 1998 1998AJ....115.1840H J/AJ/114/1458 : The Carina Dwarf (Mighell 1997) Galaxies, photometry Photometry, UBV galaxies: evolution galaxies: stellar content We have analyzed deep B and V photometry of the Carina dwarf spheroidal galaxy reaching below the old main-sequence turnoff to V~25. Using simulated color-magnitude diagrams to model a range of star formation scenarios, we have extracted a detailed, global star formation history. Carina experienced three significant episodes of star formation at ~15, 7, and 3Gyr. Contrary to the generic picture of galaxy evolution, however, the bulk of star formation, at least 50%, occurred during the episode 7Gyr ago, which may have lasted as long as 2Gyr. For unknown reasons, Carina formed only 10%-20% of its stars at an ancient epoch and then remained quiescent for more than 4 Gyr. The remainder (~30%) formed relatively recently, only 3Gyr ago. Interest in the local population of dwarf galaxies has increased lately because of their potential importance in the understanding of faint galaxy counts. We surmise that objects like Carina, which exhibits the most extreme episodic behavior of any of the dwarf spheroidal companions to the Galaxy, are capable of contributing to the observed excess of blue galaxies at B~24 only if the star formation occurred instantaneously.
Field 1 06 39 53 -50 56 59 Field 2 06 40 07 -50 52 52 Field 3 06 40 42 -50 52 18
Field 1 photometry Field 2 photometry Field 3 photometry Field Field number --- Seq Sequential number --- Xpos X position number=1 X and Y positions origin is the down left corner of the field. North to the top and west to the right. (1pix=0.58") pix Ypos Y position number=1 X and Y positions origin is the down left corner of the field. North to the top and west to the right. (1pix=0.58") pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag James Marcout, Patricia Bauer CDS 1998 Aug 12 UNKNOWN UNKNOWN Copied from ftp://ra.astro.lsa.umich.edu/pub/get/denise/carina.phot J_AJ_115_1840.xml Dwarf Cepheids in the Carina dwarf spheroidal galaxy. J/AJ/115/1856 J/AJ/115/1856 Dwarf Cepheids in Carina Dwarf Cepheids in the Carina dwarf spheroidal galaxy. M Mateo D Hurley-Keller J Nemec Astron. J. 115 1856 1998 1998AJ....115.1856M Photometry, UBV Stars, variable delta Scuti galaxies: dwarf We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, & Lutz (1994, Cat. <J/AJ/108/222> and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.
Properties of newly discovered variable stars in Carina [MHN98] Variable name (V1 to V20), [MHN98] VNN in Simbad --- Field Field number --- RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign (B1950.0) --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec <Vmag> Average V magnitude mag <Bmag> Average B magnitude mag <V>-<B> <V>-<B> colour index mag Per Period d E0 Approximate time of minimum light d DVmag DVmag mag Mode Mode number=1 F: stars pulsating in the fundamental mode O: overtone pulsators ?: cases in which the mode is uncertain --- V1 BV photometry V2 BV photometry V3 BV photometry V4 BV photometry V5 BV photometry V6 BV photometry V7 BV photometry V8 BV photometry V9 BV photometry V10 BV photometry V11 BV photometry V12 BV photometry V13 BV photometry V14 BV photometry V15 BV photometry V16 BV photometry V17 BV photometry V18 BV photometry V19 BV photometry V20 BV photometry Field Field number --- Band Band --- HJD Heliocentric Julian date d mag Magnitude in Band filter mag e_mag rms uncertainty on mag mag James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_115_1856.xml DIRECT distances to nearby galaxies using detached eclipsing binaries and Cepheids. II. Variables in the field M31A. J/AJ/115/1894 J/AJ/115/1894 Eclipsing binaries and Cepheids in M31A field DIRECT distances to nearby galaxies using detached eclipsing binaries and Cepheids. II. Variables in the field M31A. K Z Stanek J Kaluzny M Krockenberger D D Sasselov J L Tonry M Mateo Astron. J. 115 1894 1998 1998AJ....115.1894S J/AJ/115/1016 : Paper I. (M31B field). (Kaluzny+ 1998) http://cfa-www.harvard.edu/~kstanek/DIRECT : Direct Project Binaries, eclipsing Photometry, UBVRI Stars, diameters Stars, variable binaries: eclipsing Cepheids distance scale galaxies: individual (M 31) stars: variables: other We have undertaken a long-term project, DIRECT, to obtain the direct distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries (DEBs) and Cepheids. While rare and difficult to detect, DEBs provide us with the potential to determine these distances with an accuracy better than 5%. The extensive photometry obtained in order to detect DEBs provides us with good light curves for the Cepheid variables. These are essential to the parallel project to derive direct Baade-Wesselink distances to Cepheids in M31 and M33. For both Cepheids and eclipsing binaries, the distance estimates will be free of any intermediate steps. As a first step in the DIRECT project, between 1996 September and 1997 January we obtained 36 full nights on the Michigan-Dartmouth-MIT Observatory 1.3m telescope and 45 full/partial nights on the F. L. Whipple Observatory 1.2m telescope to search for DEBs and new Cepheids in the M31 and M33 galaxies. In this paper, second in a series, we present the catalog of variable stars, most of them newly detected, found in the field M31A [({alpha},{delta})=(11.34{deg}, 41.73{deg}), J2000.0]. We have found 75 variable stars: 15 eclipsing binaries, 43 Cepheids, and 17 other periodic, possible long-period or nonperiodic variables. The catalog of variables, as well as their photometry and finding charts, is available via anonymous ftp and the World Wide Web. The CCD frames are available upon request.
DIRECT eclipsing binaries in M31A M31A Name (DIRECT VNNNN M31A in Simbad) --- RAdeg Right ascension (J2000.0) deg DEdeg Declination (J20000) deg Js Variability index (Paper I, eq. (8)) --- Per Period d Vmax V magnitude at maximum brightness mag Imax Maximum I magnitude mag Rad1 Radius of the primary component number=1 The radii are in units of the orbital separation. --- Rad2 Radius of the secondary component number=1 The radii are in units of the orbital separation. --- i Inclination angle deg e Eccentricity --- Com Comment number=2 V4636 D31A, with period P=8.181 days, is a good detached eclipsing binary (DEB) candidate, with significant eccentricity. V1555 D31A was found as V6913 D31B in Paper I, with identical period, V_max_=20.63 and I_max_=20.06. --- DIRECT Cepheids in M31A M31A Name (DIRECT VNNNN M31A in Simbad) --- RAdeg Right ascension (J2000.0) deg DEdeg Declination (J2000.0) deg Js Variability index --- Per Period d <V> Flux-weighted mean V magnitude mag <I> Flux-weighted mean I magnitude mag Amp Amplitude of the variation mag Com Comments number=1 Ma97: Magnier et al., Cat. <J/A+AS/126/401>, [MAP97] in Simbad Variable V2276 D31A (Ma97 108) was found as V7553 D31B in Paper I, with period P=9.482 days, <V>=20.93, and <I>=19.77. --- DIRECT other periodic variables in M31A DIRECT miscellaneous variables in M31A M31A Name (DIRECT VNNNN M31A in Simbad) --- RAdeg Right ascension (J2000.0) deg DEdeg Declination (J2000.0) deg Js Variability index --- Per Period (only in table3.dat) d Vbar Error-weighted mean V magnitude mag Ibar Error-weighted mean I magnitude mag e_Vmag Standard deviation in the V band mag e_Imag Standard deviation in the I band mag Com Comments number=1 Variables V3222, V541 and V11 of table4 where also found in Paper I. --- Light curves of eclipsing binaries in M31A Light curves of Cepheids in M31A Light curves of other periodic variables in M31A Light curves of miscellaneous variables in M31A M31A Name (VNNNN) --- Band Band --- HJD Heliocentric Julian date d Mag Magnitude in the band (I or V) mag e_Mag rms uncertainty on Mag mag James Marcout, Patricia Bauer CDS 1998 Aug 12 UNKNOWN UNKNOWN From AJ electronic version J_AJ_115_1894.xml RR Lyrae variables in the inner halo. I. Photometry. J/AJ/115/193 J/AJ/115/193 RR Lyrae V light curves RR Lyrae variables in the inner halo. I. Photometry. A C Layden Astron. J. 115 193 1998 1998AJ....115..193L II/214 : Combined General Catalogue of Variable Stars (Kholopov+ 1998) Photometry, CCD Stars, variable Galaxy: halo Galaxy: stellar content stars: distances stars: Population II stars: variables: other I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.
Individual photometric observations Star Star name --- HJD Heliocentric Julian date of mid-observation d Phase Derive photometric phase --- Vmag Johnson V magnitude mag e_Vmag rms uncertainty on Vmag mag Run Observing run number number=1 1: 1993 Jan 8-9 2: 1993 Apr 9-13 3: 1993 May 20-22, 26 4: 1993 Aug 6-8 5: 1993 Aug 28-31 6: 1993 Sep 28 7: 1993 Oct 27-29, Nov 2 8: 1994 June 17-20, 26-27 --- Derived light-curve parameters Star Star name --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec AV Interstellar absorption in V band mag Per Adopted period d e_Per rms uncertainty on Per (99: e_Per>10-3d) 10-5d n_Per Origin of the period number=1 1: P_GCVS4_ (Cat. <II/214>) was adopted for the star 2: the adopted period is at most a few percent away from P_GCVS4_ (Cat. <II/214>) 3: the adopted period is farther away from P_GCVS4_ (Cat. <II/214>), and hence more questionable --- <Vmag> Average V magnitude mag Emax Epoch (Julian date) at maximum light d e_Emax rms uncertainty on Emax d Nobs Number of observations --- Six light-curve templates Phase Phase --- V1 Template 1 V magnitude --- V2 Template 2 V magnitude --- V3 Template 3 V magnitude --- V4 Template 4 V magnitude --- V5 Template 5 V magnitude --- V6 Template 6 V magnitude --- James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_115_193.xml New variables in the Sloan Digital Sky Survey calibration fields. J/AJ/115/296 J/AJ/115/296 SDSS new variables New variables in the Sloan Digital Sky Survey calibration fields. A A Henden R C Stone Astron. J. 115 296 1998 1998AJ....115..296H II/214 : General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1998) Photometry Stars, variable Cepheids stars: variables: other The US Naval Observatory 0.2m Flagstaff Astrometric Scanning Transit Telescope (FASTT) was used to obtain astrometric information in 16 equatorial fields in support of the Sloan Digital Sky Survey (SDSS). Each field is approximately 7.6{deg}x3.2{deg} in size and was scanned ~10 times with overlapping CCD strip scans; star positions accurate to +/-50mas in each coordinate and magnitudes good to +/-0.011mag were determined. As an ancillary project, this database was searched for new variables, and the results of that search are presented here. Approximately 1500 new variables have been discovered, and accurate coordinates for ~100 previously identified variables and suspected variables are given.
SDSS calibration regions Region Region designation --- RA1h Right ascension (J2000.0), lower limit h RA1m Right ascension (J2000.0), lower limit min RA1s Right ascension (J2000.0), lower limit s RA2h Right ascension (J2000.0), upper limit h RA2m Right ascension (J2000.0), upper limit min RA2s Right ascension (J2000.0), upper limit s DE1- Declination sign, lower limit --- DE1d Declination (J2000.0), lower limit deg DE1m Declination (J2000.0), lower limit arcmin DE1s Declination (J2000.0), lower limit arcsec DE2d Declination (J2000.0), upper limit deg DE2m Declination (J2000.0), upper limit arcmin DE2s Declination (J2000.0), upper limit arcsec Size1 Angular size deg --- --- Size2 Angular size deg Nstar Number of stars --- Nobs2 Estimated number of stars for full sampling in the four regions with only partial parameters --- RFmag Limiting magnitude R_F_ mag GLON Galactic longitude deg GLAT Galactic latitude deg Nobs Mean number photometric observations of each star --- Nvar1 Number of variables found subject from 3{sigma} --- Nvar2 Number of variables found subject from 3{sigma}/FWHM --- Nvar True number of variables found subject --- Variable stars HS HS identification number --- n_HS *: variable also appears in table3.dat --- SDSS Star designation (ANNNNNNNN) --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec RFmag Mean R_F_ magnitude mag e_RFmag rms uncertainty on RFmag mag x/y Ratio of the FWHM in x and y --- e_x/y rms uncertainty on x/y --- Nobs Number of times each variable was observed --- Type Classification for the variable --- Note Notes pertaining to the nature of the variability --- Known variable stars Name Star name --- SDSS Star designation (ANNNNNNNN) --- n_SDSS *: Star does not appear in table2.dat --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec DPos Positional error between the GCVS (Cat. <II/139>) and FASTT positions arcmin Type Classification type --- magMax Maximum magnitude Mag mag magMin Minimum magnitude Mag mag Mag Magnitude filter --- RFmag Mean R_F_ magnitude mag JD Epoch of observation d Per Period d Patricia Bauer CDS 1998 Mar 10 UNKNOWN UNKNOWN Copied from electronic Astronomical Journal version J_AJ_115_296.xml Mass segregation in young Large Magellanic Cloud clusters. I. NGC 2157. J/AJ/115/592 J/AJ/115/592 VI photometry of NGC 2157 Mass segregation in young Large Magellanic Cloud clusters. I. NGC 2157. P Fischer C Pryor S Murray M Mateo T Richtler Astron. J. 115 592 1998 1998AJ....115..592F VII/183 : Cluster System of the LMC (Kontizas+ 1990) Clusters, open Magellanic Clouds Photometry, VRI galaxies: star clusters globular clusters: individual (NGC 2157) Magellanic Clouds We have carried out Wide Field Planetary Camera 2 V- and I-band imaging of the young LMC cluster NGC 2157. Construction of a color-magnitude diagram and isochrone fitting yield an age of {tau}=10^8^yr, a reddening E(B-V)=0.1, and a distance modulus of 18.4mag. Our data cover the mass range 0.75M_{sun}_<=m<=5.1M_{sun}_. We find that the cluster mass function changes significantly from the inner regions to the outer regions, becoming steeper (larger number of low-mass stars relative to high-mass stars) at larger radii. The age of NGC 2157 is comparable to its two-body relaxation timescale only in the cluster core. The observed steepening of the mass function at larger radii is therefore most likely an initial condition of the cluster stars. Such initial conditions are predicted in models of cluster star formation in which dissipative processes act more strongly upon more massive stars.
HST NGC 2157 05 57 35.0 -69 11 48
Cluster Planerary Camera (PC) photometry Cluster Wide Field Planerary Camera 2 (WF2) photometry Cluster WF3 photometry Cluster WF4 photometry Background PC photometry Background WF2 photometry Background WF3 photometry Background WF4 photometry Seq Sequential number --- xpos x position number=1 The cluster center is located in the Planetary Camera (PC) frame. pix ypos y position number=1 The cluster center is located in the Planetary Camera (PC) frame. pix V0 Dereddenned V magnitude number=2 Reddening correction of E(B-V)=0.1. mag e_V0 rms uncertainty on V0 mag (V-I)0 Dereddenned V-I index number=2 Reddening correction of E(B-V)=0.1. mag e_(V-I)0 rms uncertainty on (V-I)0 mag James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_115_592.xml Kinematics of the Hercules supercluster J/AJ/115/6 J/AJ/115/6 Hercules supercluster kinematics Kinematics of the Hercules supercluster P Barmby J P Huchra Astron. J. 115 6 1998 1998AJ....115....6B VII/99 : Radial Velocities of Galaxies (Palumbo+ 1986) VII/112 : RC2 Catalogue (de Vaucouleurs+ 1976) VII/155 : RC3 Catalogue (de Vaucouleurs+ 1991) VII/172 : First Byurakan Survey (FBS) (Markarian+, 1989) J/A+AS/109/537 : Redshift survey of faint galaxies (Hopp+, 1995) Clusters, galaxy Photometry, CCD Radial velocities cosmology: observations dark matter galaxies: clusters: individual (Hercules) The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the KMM mixture-modeling algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, & Huchra (1982ApJ...257..323B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.
*Galaxies in the Hercules supercluster Name Galaxy name --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Rmag R magnitude mag HV Heliocentric velocity km/s e_HV rms uncertainty on HV km/s MType Morphological type --- r_HV Velocity source, see refs.dat --- CCD photometry for A2151 galaxies Name Galaxy name --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Bmag B magnitude mag B-R B-R colour index mag References quoted in Table 1 RefCode Reference code --- Text Text of reference (including the 19-digit bibcode) --- table1.tex LaTeX Version of Table 1 table1.ps Postscript version of Table 1 Patricia Bauer CDS 1998 Mar 05 UNKNOWN UNKNOWN * 05-Mar-1998: Copied from the electronic version of AJ http://cdsaas.u-strasbg.fr:2001/AJ/journal/contents/v115n1.html * 02-Jun-1998 (from Pauline Barmby, <pbarmby@cfa.harvard.edu>) Table 1, Galaxies in the Hercules Supercluster, had several errors, including typographical errors in coordinates, object misidentifications, and duplicate entries. We have corrected these errors and determined that they not do not affect the conclusions of the paper. A corrected version of the table, containing 458 galaxies with velocities (171 new velocities) is available in the electronic version of the paper. We thank M. Schmitz for bringing some of the errors to our attention. J_AJ_115_6.xml The Global Kinematics of the Globular Clutser M15 J/AJ/115/708 J/AJ/115/708 Radial Velocities in the Field of M15 The Global Kinematics of the Globular Clutser M15 G A Drukier S D Slavin H N Cohn P M Lugger R C Berrington B W Murphy P O Seitzer Astron. J. 115 708 1998 1998AJ....115..708D Clusters, globular Radial velocities These tables give the mean radial velocities for 591 stars in the vicinity of the globular cluster M15 (NGC 7078). 230 of these are members of the cluster, the remaining 361 are most likely non-members, although the membership, or otherwise, of the faintest stars with velocities near that of the cluster was impossible to determine. The radial velocities were measured using the Hydra multi-object spectrograph on the WIYN telescope. For cluster members, the median uncertainty is 0.3 km/s.
Velocities of members RAh Hours of right ascension h RAm Minutes of right ascension min RAs Seconds of right ascension s DEd Degrees of declination deg DEm Minutes of declination arcmin DEs Seconds of declination arcsec ID Identifier --- Vmag V magnitude --- Number Number of observations --- RV Radial velocity km/s e_RV Uncertainty in Radial Velocity km/s Prob Probability of chi(1) --- Alt_ID Alternative Identification --- Note Note on variability(2) --- Velocities of non-members RAh Hours of right ascension h RAm Minutes of right ascension min RAs Seconds of right ascension s DEd Degrees of declination deg DEm Minutes of declination arcmin DEs Seconds of declination arcsec ID Identifier --- Vmag V magnitude --- Number Number of observations --- RV Radial velocity km/s e_RV Uncertainty in Radial Velocity km/s Prob Probability of chi(1) --- G.A. Drukier Indiana University 1998 Feb 16 Data obtained with the WIYN telescope. The WIYN Observatory is a joint facility of the University of Wisconsin, Indiana University, Yale University and the National Optical Astronomy Observatory. UNKNOWN UNKNOWN Stars with names starting with K are from Kustner (1921). Those with AC are from Auriere & Cordoni (1981). The others with single alphabetical prefixes are from Sandage (1970). Those with Geb are from Gebhardt (1997). The numerical identifications are our own. J_AJ_115_708.xml Deep optical imaging of the bright Seyfert galaxy NGC 5548: a long, very low surface brightness tail. J/AJ/116/102 J/AJ/116/102 NGC 5548 BR photometry Deep optical imaging of the bright Seyfert galaxy NGC 5548: a long, very low surface brightness tail. J A Tyson P Fischer P Guhathakurta P McIlroy R Wenk J Huchra L Macri L Neuschaefer V Sarajedini K Glazebrook K Ratnatunga R Griffiths Astron. J. 116 102 1998 1998AJ....116..102T J/A+A/314/43 : NGC 5548 Profile variability (Kollatschny+ 1996) Galaxies, Seyfert Photometry galaxies: clusters: general galaxies: individual (NGC 5548) galaxies: Seyfert Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.
BR photometry in the NGC 5548 field [TFG98] Star name (NGC 5548-NN) --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag B-R B-R colour index mag e_B-R rms uncertainty on B-R mag James Marcout, Patricia Bauer CDS 1998 Nov 09 From AJ electronic version J_AJ_116_102.xml Galaxy alignments in the Pisces-Perseus supercluster revisited. J/AJ/116/1094 J/AJ/116/1094 MAPS-PP catalog of galaxies Galaxy alignments in the Pisces-Perseus supercluster revisited. J E Cabanela G Aldering Astron. J. 116 1094 1998 1998AJ....116.1094C VII/193 : The CfA Redshift Catalogue (ZCAT) (Huchra+ 1995) VII/198 : Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997) J/A+A/286/17 : 21cm obs. of galaxies in Psc-Per Supercl. (Seeberger+ 1994) J/AJ/105/1271 : Pisces-Perseus supercluster. VI (Giovanelli+, 1993) J/AJ/105/1251 : Pisces-Perseus supercluster. V. (Wegner+, 1993) http://aps.umn.edu/ : APS databases Clusters, galaxy Galaxy catalogs Magnitudes Morphology galaxies: formation galaxies: structure A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.
The MAPS-PP catalog of galaxies: APS parameters Source Source name number=1 Some rasters of multiple merged galaxies were split when the individual galaxies were large enough to make the diameter cut. These split rasters are indicated by an A, B, or C suffix. --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign (1950.0) --- DEd Declination (150.0) deg DEm Declination (150.0) arcmin DEs Declination (150.0) arcsec Eps Ellipticity of the galaxy, from the passband indicated by the galaxy name --- e_Eps rms uncertainty on Eps --- PA Position angle from the passband indicated by the galaxy name deg e_PA rms uncertainty on PA deg aO O-plate major axis arcsec aE E-plate major axis arcsec mO O-plate magnitude mag mE E-plate magnitude mag mO-mE Difference magnitude O-E mag chi2O O chi-2 value --- chi2E E chi-2 value --- Cross-identifications and additional galaxy parameters Source Source designation number=1 Some rasters of multiple merged galaxies were split when the individual galaxies were large enough to make the diameter cut. These split rasters are indicated by an A, B, or C suffix. --- Name Catalog name --- cz Heliocentric radial velocity km/s Ttype Morphological Type number=2 Morphological types in zcat: -7 = Unclassified Elliptical -5 = E, and dwarf E -4 = E/SO -3 = L-, SO- -2 = L, SO -1 = L+, SO+ 0 = SO/a, SO-a 1 = Sa 2 = Sab 3 = Sb 4 = Sbc 5 = Sc 6 = Scd 7 = Sd 8 = Sdm 9 = Sm, Magellanic Spiral 10 = Im, Irr I, Magellanic Irregular, Dwarf Irregular 11 = Compact Irregular, Extragalactic HII Region 15 = Peculiar, Unclassifiable 20 = S..., Sc-Irr, Unclassified Spiral 99 --- Cat ZCAT number or other catalogs number=3 Source numbers are identical to ZCAT (Cat. <VII/193> source numbers for values less than 100 101: Giovanelli & Haynes, 1993, Cat. <J/AJ/105/1271> 102: Giovanelli & Haynes H{alpha} observations 103: Sakai et al., 1994AJ....108...33S 200: RC3, Cat. <VII/155> 301: W91CL, Mark III catalog (Cat. <VII/198>) 302: W91PP, Mark III catalog (Cat. <VII/198>) 303: WCF, Mark III catalog (Cat. <VII/198>) --- AV Galactic extinction mag North Direction of the true North, relative to machine axes deg Rridge Radius of the closest ridgeline point deg r10 r_10_ surface density in galaxies/deg^2^ number=4 The angular separation between each galaxy and its tenth closest neighbor, r_10_, was determined. Assuming there are 11 galaxies within a circle of radius r_10_, the number of galaxies per square degree is readily computed. deg-2 OFlag O quality flag number=5 The absolute values of the quality flags indicates: 1: good fit 2: prominent dust lane or non-elliptical isodensity affects fit 3: irregular appearance affects fit 4: prominent spiral pattern affects fit 5: prominent galaxy bar affects fit If the sign of the flag is negative, the magnitudes include catalog or estimate magnitudes --- EFlag E quality flag number=5 The absolute values of the quality flags indicates: 1: good fit 2: prominent dust lane or non-elliptical isodensity affects fit 3: irregular appearance affects fit 4: prominent spiral pattern affects fit 5: prominent galaxy bar affects fit If the sign of the flag is negative, the magnitudes include catalog or estimate magnitudes --- James Marcout, Patricia Bauer CDS 1998 Nov 19 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_1094.xml Recent star formation in Shapley constellation III in the Large Magellanic Cloud J/AJ/116/1275 J/AJ/116/1275 UBV photometry in 5 fields of the LMC Recent star formation in Shapley constellation III in the Large Magellanic Cloud A E Dolphin D A Hunter Astron. J. 116 1275 1998 1998AJ....116.1275D J/MNRAS/260/782 : CCD photometry of NGC 2004 and 2100 (Balona+ 1993) Magellanic Clouds Photometry, CCD Photometry, UBV Populations, stellar galaxies: formation galaxies: stellar content Magellanic Clouds We present UBV photometry of four fields within Shapley Constellation III and one field on the edge of the shell. Our fields cover roughly 20% of the region, mostly in the southern half. Determinations are made of ages of the fields, the star formation densities, and the initial mass function (IMF) slopes.
Field LH 77 05 30 40.8 -66 55 33 Field NGC 2027 05 35 04.7 -66 55 07 Field SL 502 05 29 00.2 -66 34 52 Field NGC 2004 05 31 10.5 -67 16 57 Field NGC 1955 05 26 08.8 -67 29 48 Field BNW 05 10 02.1 -66 36 23 Field BSE 05 40 12.7 -67 11 46
LH 77 Field (5 30 41.7 -66 56 37 (1975)) SL 502 Field (5 28 59.8 -66 36 00 (1975)), ([SL63] 502 in Simbad) NGC 2027 Field (5 35 05.8 -66 56 01 (1975)) NGC 2004 Field (5 31 12.8 -67 18 00 (1975)) NGC 1955 Field (5 26 11.7 -67 31 02 (1975)) Background SE Field (5 40 15.0 -67 12 29 (1975)) Background NW Field (5 10 00.7 -66 38 12 (1975)) Xpos X position number=1 North is to the right, large Xpos; East is up, small Ypos. In Simbad, sources are identified as [DH98] LH 77 XXXX.xxx-YYYY.yyy, [DH98] NGC NNNN XXXX.xxx-YYYY.yyy, [DH98] SL 502 XXXX.xxx-YYYY.yyy, [DH98] BWW XXXX.xxx-YYYY.yyy pix Ypos Y position number=1 North is to the right, large Xpos; East is up, small Ypos. In Simbad, sources are identified as [DH98] LH 77 XXXX.xxx-YYYY.yyy, [DH98] NGC NNNN XXXX.xxx-YYYY.yyy, [DH98] SL 502 XXXX.xxx-YYYY.yyy, [DH98] BWW XXXX.xxx-YYYY.yyy pix Umag U magnitude mag e_Umag rms uncertainty on Umag mag Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag James Marcout, Patricia Bauer CDS 1998 Nov 19 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_1275.xml Near-infrared photometric studies of RZ Cassiopeiae. J/AJ/116/1447 J/AJ/116/1447 RZ Cas JK light curves Near-infrared photometric studies of RZ Cassiopeiae. W P Varricatt N M Ashok T Chandrasekhar Astron. J. 116 1447 1998 1998AJ....116.1447V Binaries, eclipsing Photometry, infrared binaries: eclipsing stars: activity stars: individual (RZ Cas) stars: spots Light curves of the Algol-type binary system, RZ Cassiopeiae, in the near-IR wavelengths J and K are obtained for the first time. The light curves are analyzed using the Wilson-Devinney model. UBV light curves of RZ Cas obtained by Chambliss are also reanalyzed using the same program. In the J and K bands, the bolometric albedo of the secondary of RZ Cas exhibited values above 0.7, whereas the theoretically expected value for such a star is 0.5. Also, the values of the secondary temperature derived from the J and K light curves are found to be less than that derived from our analysis of the optical light curves as well as from the previous studies in the optical photometric bands. We have attempted to model these effects with a dark spot on the secondary of RZ Cas. The J-band light curve gave a better fit with a cool dark spot on the secondary. Another possible reason for the above mentioned effects is a gas stream from the lobe-filling secondary to the primary star. The magnitudes and colors of the individual components are derived from the observed light curves and the light contributions from the stars derived from the light curve analysis. The primary is found to be an A3 V star as observed by previous investigators. The secondary is classified as K0K4 IV from the derived colors. Seven epochs of primary minima and 3 epochs of secondary minima are obtained from the observations. Because of the increased depths of the secondary eclipse in the infrared bands, the moments of minima are calculated with nearly the same accuracy as that of the primary minima. All the secondary minima are found to occur at phase 0.5. None of the observed primary minima are flat as found by many observers before at optical wavelengths. The colors of the system at the minima obtained by us confirm that the system is partially eclipsing.
RZ Cas HD 17138 02 48 55.5 +69 38 03
J-band light curve of RZ Cassiopeiae K-band light curve of RZ Cassiopeiae HJD Heliocentric Julian date d Phase Phase --- Dmag Differential magnitude mag James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_1447.xml Star formation in and evolution of the blue compact dwarf galaxy UGC 6456 determined from Hubble space telescope images J/AJ/116/146 J/AJ/116/146 UGC 6456 HST photometry Star formation in and evolution of the blue compact dwarf galaxy UGC 6456 determined from Hubble space telescope images R Lynds E Tolstoy E J O'Neil Jr. D A Hunter Astron. J. 116 146 1998 1998AJ....116..146L J/A+AS/111/527 : CCD photometry of 11 dwarf irregular galaxies (Hopp+, 1995) Galaxies, photometry Photometry, CCD color-magnitude diagrams (HR diagram) galaxies: dwarf galaxies: individual (UGC 6456) galaxies: irregular stars: AGB and post-AGB Photometry on the UVI system has been performed on the resolved stellar content of the blue compact dwarf galaxy UGC 6456 using Wide Field Planetary Camera 2 (WFPC2) images obtained with the Hubble Space Telescope. The resulting color-magnitude diagram (CMD) goes to about V=27.5 and reveals not only a young population of blue main-sequence stars and blue and red supergiants, but also an older evolved population of red giants and a fairly well represented asymptotic giant branch. The distance to the galaxy is estimated from the tip of the red giant branch to be 4.5Mpc, placing it about 1.5Mpc farther away than the major members of the M81 Group, with which it is usually associated. The youngest stars are generally associated with H ii regions shown on our Halpha image and are largely confined to the 745pc field of our PC images. A comparison of their distribution in the CMD with theoretical isochrones suggests ages from 4 to 10Myr. The population of older stars is found throughout all WFPC2 camera fields and seems to show an elliptical distribution with an aspect ratio of about 2.4 and an exponential falloff in surface density with distance from a center of symmetry that is not far from the centroid of the youngest stars. Theoretical modeling of the CMD at a metallicity of Z=0.001 suggests star formation in the age interval 1-2Gyr, a strong burst in the interval 600-800Myr, and a lower rate of star formation up to the present. The evidence is compatible with a scenario beginning with the formation of a population of low-metallicity stars, enriching a major residual of prestellar material that subsequently fueled an active episode of star formation. That burst of star formation must have been particularly spectacular and may be related to the activity we now see in the distant blue dwarf galaxies revealed in deep imaging.
HST UGC 6456 VIIZw 403 11 24 35.9 +79 16 02
The Galaxy Photometry [LTO98] Identification number --- xpos x position number=1 Coordinates relative to Figure 1. North is 115{deg} clockwise from the top. The coordinates origin (0,0) is the bottom left corner. 1 pix = 0.1". pix ypos y position number=1 Coordinates relative to Figure 1. North is 115{deg} clockwise from the top. The coordinates origin (0,0) is the bottom left corner. 1 pix = 0.1". pix F336W F336W magnitude number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag e_F336W rms uncertainty on F336W number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag F555W F555W magnitude number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag e_F555W rms uncertainty on F555W number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag F814W F814W magnitude number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag e_F814W rms uncertainty on F814W number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag F336W-F555W F336W-F555W colour index number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag e_F336W-F555W rms uncertainty on F336W-F555W number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag F555W-F814W F555W-F814W colour index number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag e_F555W-F814W rms uncertainty on F555W-F814W number=2 A magnitude of 100.00 indicates that the star was not measured through that filter mag James Marcout, Patricia Bauer CDS 1998 Sep 22 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_146.xml Dynamics of cD clusters of galaxies. III. Redshift data for 11 Abell clusters. J/AJ/116/1529 J/AJ/116/1529 cD clusters of galaxies. III. Dynamics of cD clusters of galaxies. III. Redshift data for 11 Abell clusters. J M Hill W R Oegerle Astron. J. 116 1529 1998 1998AJ....116.1529H J/AJ/106/831 : cD clusters of galaxies. I. (Hill+, 1993) Oegerle and Hill, Paper II. 1994AJ....107..857O Clusters, galaxy Redshifts Spectroscopy cosmology: miscellaneous galaxies: clusters: general galaxies: distances and redshifts We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.
A779 redshift data (table 2) A1691 redshift data (table 3) A1749 redshift data (table 4) A1757 redshift data (table 5) A1837 redshift data (table 6) A1927 redshift data (table 7) A2067 redshift data (table 8) A2079 redshift data (table 8) A2089 redshift data (table 10) A2199 redshift data (table 11) A2666 redshift data (table 12) HO98 Sequential number number=1 [HO98] ACO NNNN NNN in Simbad --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec cz Heliocentric velocity km/s e_cz rms uncertainty on cz km/s Name Other name --- Note Notes number=2 E: the velocity comes from measurements of emission lines only, rather than the cross-correlation of the absorption spectra A: presence of absorption in the Balmer series NM: foreground or background galaxy that is not a velocity member of the cluster cD: central cD galaxy. Is followed by the number of repeated independent observations of the cD redshift --- lines Presence of emission lines or comments --- James Marcout, Patricia Bauer CDS 1998 Dec 08 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_1529.xml Environments of Redshift Survey Compact Groups of galaxies. J/AJ/116/1573 J/AJ/116/1573 Redshift Survey Compact Groups Environments of Redshift Survey Compact Groups of galaxies. E J Barton R R De Carvalho M J Geller Astron. J. 116 1573 1998 1998AJ....116.1573B VII/193 : The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995) J/AJ/116/1 : Southern Sky Redshift Survey (Da Costa+, 1998) Clusters, galaxy Magnitudes Redshifts galaxies: clusters: general galaxies: distances and redshifts galaxies: interactions Redshift Survey Compact Groups (RSCGs) are tight knots of N>=3 galaxies selected from the CfA2+SSRS2 redshift survey. The selection is based on physical extent and association in redshift space alone. We measured 300 new redshifts of fainter galaxies within 1h^-1^Mpc of 14 RSCGs to explore the relationship between RSCGs and their environments. Thirteen of 14 RSCGs are embedded in overdense regions of redshift space. The systems range from a loose group of five members to an Abell cluster. The remaining group, RSCG 64, appears isolated. RSCGs are isolated and distinct from their surroundings to varying degrees, as are the Hickson compact groups. Among the 13 embedded RSCGs, three are distinct from their general environments (RSCG 9, RSCG 11, and RSCG 85).
Catalog of Redshifts Surrounding RSCGs RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec mZU Approximate magnitude on Zwicky scale mag HRV Heliocentric velocity km/s e_HRV rms uncertainty on HRV km/s Source Source number=1 Z = ZCAT (Cat. <VII/193>), F = new FAST spectrum --- ZCAT Name in ZCAT (Cat. <VII/193>) --- Com Comments number=2 "env. of 73" indicates that the galaxy is in the environment of RSCG 73, which we identified with the friends-of-friends algorithm --- table3.tex LaTeX version of table 3 James Marcout, Patricia Bauer CDS 1998 Dec 08 UNKNOWN UNKNOWN //cfa0.harvard.edu/pub/barton/ J_AJ_116_1573.xml Globular cluster photometry with the Hubble Space Telescope. VII. Color gradients and blue stragglers in the central region of M30 from Wide Field Planetary Camera 2 observations. J/AJ/116/1757 J/AJ/116/1757 M30 UBV photometry Globular cluster photometry with the Hubble Space Telescope. VII. Color gradients and blue stragglers in the central region of M30 from Wide Field Planetary Camera 2 observations. P Guhathakurta Z T Webster B Yanny D P Schneider J N Bahcall Astron. J. 116 1757 1998 1998AJ....116.1757G J/AJ/107/1745 : HST UVI photometry of M15. II. (Yanny+, 1994) J/AJ/108/1786 : Blue stragglers + variable stars in M3 (Guhathakurta+, 1994) J/AJ/113/669 : Stars in M13 core (Cohen+ 1997) Guhathakurta et al., Paper I. 1992AJ....104.1790G Yanny et al., Paper II. 1994AJ....107.1745Y, Cat. <J/AJ/107/1745> Guhathakurta et al., Paper III. 1994AJ....108.1786G, Cat. <J/AJ/108/1786> Yanny et al., Paper IV. 1994ApJ...435L..59Y Guhathakurta et al., Paper V. 1996AJ....111..267G Cohen et al., Paper VI. 1997AJ....113..669C, Cat. <J/AJ/113/669> Clusters, globular Photometry, UBV Stars, blue blue stragglers color-magnitude diagrams (HR diagram) globular clusters: individual (M 30, NGC 7099) stars: evolution stars: luminosity function, mass funtion We present F555W (V), F439W (B), and F336W (U) photometry of 9507 stars in the central 2' of the dense, post-core-collapse cluster M30 (NGC 7099) derived from Hubble Space Telescope Wide Field Planetary Camera 2 images. These data are used to study the mix of stellar populations in the central region of the cluster. Forty-eight blue straggler stars are identified; they are found to be strongly concentrated toward the cluster center. The specific frequency of blue stragglers, F_BSS_=N(BSS)/N(V<V_HB_+2), is 0.25+/-0.05 in the inner region of M30 (r<20"), significantly higher than the frequency found in other clusters: F_BSS_=0.05-0.15. The shape of M30's blue straggler luminosity function resembles the prediction of the collisional formation model, and is inconsistent with the binary merger model of Bailyn & Pinsonneault (1995ApJ...439..705B). An unusually blue star (B=18.6, B-V=-0.97), possibly a cataclysmic variable based on its color, is found about 1.2" from the crowded cluster center; the photometric uncertainty for this star is large, however, because of the presence of a very close neighbor. Bright red giant stars (B<16.6) appear to be depleted by a factor of 2-3 in the inner r<10" relative to fainter giants, subgiants, and main-sequence turnoff stars (95% significance). We confirm that there is a radial gradient in the color of the overall cluster light, going from B-V~0.82 at r~1' to B-V~0.45 in the central 10". The central depletion of the bright red giants is responsible for about half of the observed color gradient; the rest of the gradient is caused by the relative underabundance of faint red main-sequence stars near the cluster center (presumably a result of mass segregation). The luminosity function of M30's evolved stars does not match the luminosity function shape derived from standard stellar evolutionary models: the ratio of the number of bright giants to the number of turnoff stars in the cluster is 30% higher than predicted by the model (3.8{sigma} effect), roughly independent of red giant brightness over the range M_V_=-2 to +2.
HST
M 30 stellar photometry and astrometry GWY Identification number number=1 Cl* NGC 7099 GWY NNNN in Simbad --- oRA Relative right ascension to star 3611 (J2000) number=2 Star 3611 position: RA=21h40min22.402s, DE=-23{deg}10'42.42" (J2000.0) arcsec oDE Relative declination to star 3611 (J2000) number=2 Star 3611 position: RA=21h40min22.402s, DE=-23{deg}10'42.42" (J2000.0) arcsec r Projected distance from the cluster centroid number=3 Cluster centroid position: RA=21h40min22.24s, DE=-23{deg}10'50.0" (J2000.0) arcsec Vmag V magnitude mag B-V B-V colour index mag U-V U-V colour index mag Patricia Bauer CDS 1998 Nov 09 UNKNOWN UNKNOWN Copied from ftp ku.sns.ias.edu J_AJ_116_1757.xml CCD photometry of the globular cluster M 53. I. Color-magnitude data and blue straggler stars. J/AJ/116/1775 J/AJ/116/1775 BV photometry of M53 CCD photometry of the globular cluster M 53. I. Color-magnitude data and blue straggler stars. S -C Rey Y -W Lee Y -I Byun M -S Chun Astron. J. 116 1775 1998 1998AJ....116.1775R V/97 : Updated 3rd Cat Variable Stars in Globular Clusters (Clement+ 1997) Clusters, globular Photometry, CCD Stars, blue blue stragglers color-magnitude diagrams (HR diagram) globular clusters: individual (M 53) The first large-format CCD color-magnitude diagram (CMD) in the B and V passbands is presented for the Galactic globular cluster M53 (NGC 5024). The observations consist of 40 pairs of B and V CCD frames with FWHM<1.2" in a pattern covering a 12'x13' region of M53. These frames were used to produce color-magnitude data for more than 20,000 stars from the tip of the red giant branch (RGB) to about 2 mag below the main-sequence turnoff (V~22). The CMD reveals a classic example of a metal-poor stellar system, with the horizontal branch (HB) predominantly blueward of the RR Lyrae instability strip and the relatively steep RGB. The blue HB of M53 does not show the blue tail phenomenon that is observed in M15. The relative age dating based on the color difference between the turnoff and the base of RGB reveals no significant age difference ({Delta}t<1Gyr) between M53 and M92. We have discovered 114 new blue straggler stars (BSSs) in the field of M53. The analysis of bright (V<19.39) BSSs clearly shows a bimodal radial distribution with a high frequency in the inner and outer regions but a distinct dip in the intermediate region. The distribution is similar to that found in M3, a globular cluster with a similar central density and concentration.
NGC 5024 M 53 13 12 55.2 +18 12 09
CCD photometry for M 53 M 53 blue straggler stars RLB/BSS Sequential number number=1 For table2.dat: Cl* NGC 5024 RLB NNNNN in Simbad For table7.dat: Cl* NGC 5024 BSS NNN in Simbad --- xpos X coordinate number=2 Positions relative to the cluster center. 1 pix = 0.22" North is down and east is to the right. pix ypos Y coordinate number=2 Positions relative to the cluster center. 1 pix = 0.22" North is down and east is to the right. pix Vmag V magnitude mag B-V B-V colour index mag HC91 Heasley & Christian (1991AJ....101..967H) number --- Identified RR Lyrae variables New RR Lyrae candidates Region Region designation number=1 A: NE region B: NW Region C: SE Region D: SW Region --- Name Name number=2 SNN : Sawyer Hogg, 1973, Cat. <V/97> designation, (Cl* NGC 5024 SAW VNNN in Simbad, table3.dat) VN: this paper designation (Cl* NGC 5024 RLB VN in Simbad, table4.dat) --- RLB RLB number --- Band Band --- mag1 Magnitude in Band at JD=2449807.872 mag mag2 Magnitude in Band at JD=2449807.895 mag mag3 Magnitude in Band at JD=2449807.939 mag mag4 Magnitude in Band at JD=2449807.965 mag mag5 Magnitude in Band at JD=2449808.796 mag mag6 Magnitude in Band at JD=2449808.881 mag mag7 Magnitude in Band at JD=2449808.932 mag mag8 Magnitude in Band at JD=2449809.007 mag mag9 Magnitude in Band at JD=2449809.046 mag mag10 Magnitude in Band at JD=2449809.065 mag mag11 Magnitude in Band at JD=2449809.113 mag James Marcout, Patricia Bauer CDS 1998 Dec 08 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_1775.xml WIYN Open Cluster Study 1: Deep Photometry of NGC 188 J/AJ/116/1789 J/AJ/116/1789 VI Photometry of NGC 188 WIYN Open Cluster Study 1: Deep Photometry of NGC 188 T von Hippel A Sarajedini Astron. J. 116 1789 1998 1998AJ....116.1789V Clusters, open Photometry We present V and I broad-band photometry on the Johnson-Kron-Cousins (Landolt 1992) system for the central 6.7' x 6.7' field of the old open cluster NGC 188. Only objects with a probability of >= 95% of being stellar based on SExtractor (Bertin & Arnouts 1996) analysis of 0.7" I-band images are presented. The resulting photometry of 750 sources spans the range from V = 14 (just above the turn-off) to V = 26. We estimate the external accuracy (tie to the Landolt system) to be <= 0.01 mag for the brightest stars (V < 17) and <= 0.032 mag for the fainter stars blueward of V-I = 2. Stars redder than V-I = 2 required an extrapolation of our standard star solution. Equatorial coordinates for equinox J2000 and epoch 1996.10 were kindly derived by Imants Platais, Yale University, using 160 reference stars from the HST Guide Star Catalog. The standard error of the coordinates is 0.14", primarily limited by the accuracy of GSC star positions.
NGC 188 VI photometry data file IAU IAU designation The IDs are based on the IAU standard system and include the name of our collaboration, WOCS (WIYN Open Cluster Study), followed by J for J2000 coordinates, and then the coordinates themselves in RA+Dec notation. For example, our first object is WOCS J0049562+851236 with coordinates RA=00:49:56.29 and Dec=+85:12:36.2 (J2000). ------------------------------------------------------------------------------- References: "UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equator.", 1992, Landolt, A.U., AJ, 104, 340 "SExtractor: Software for source extraction.", 1996, Bertin, E., Arnouts, S., 1996, A&AS, 117, 393 --- RAh Right Ascension hours (J2000) h RAm Right Ascension minutes (J2000) min RAs Right Ascension seconds (J2000) s DEd Declination degrees (J2000) deg DEm Declination minutes (J2000) arcmin DEs Declination seconds (J2000) arcsec X CCD X position pix Y CCD Y position pix V V magnitude mag u_V IRAF estimated V magnitude error mag o_V number of V-bandpass measurements --- I I magnitude mag u_I IRAF estimated I magnitude error mag o_I number of I-band measurements --- prob stellar classification probability % Ted von Hippel NOAO modified by James E. Gass SSDOO/ADC 1998 Oct 27 J_AJ_116_1789.xml Ultraviolet Imaging Telescope Observations of the Magellanic Clouds J/AJ/116/180 J/AJ/116/180 UIT Observations of the Magellanic Clouds Ultraviolet Imaging Telescope Observations of the Magellanic Clouds J W Parker J K Hill R H Cornett J Hollis E Zamkoff R C Bohlin R W O'Connell S G Neff M S Roberts A M Smith T P Stecher Astron. J. 116 180 1998 1998AJ....116..180P J/AJ/113/1011 : Catalog of UIT photometry for the SMC which was discussed and analyzed by Cornett et al. =1997AJ....113.1011C Atlases Clusters, open Magellanic Clouds Photometry, ultraviolet Stars, blue Stars, early-type Stars, OB Surveys Ultraviolet This is a catalog of far-ultraviolet (FUV: 1300-1800 A) magnitudes derived from point spread function photometry for 37,333 stars in the LMC (FUV magnitudes for 11,306 stars in the SMC were presented in the paper by Cornett et al. =1997AJ....113.1011C), with an observational completeness limit of m_UV~15 mag and a detection limit of m_UV~17.5. The average uncertainty in the photometry is ~0.1 mag. This catalog was referred to, but did not appear in, the printed paper. The sources of the photometry are wide-field FUV images obtained by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 (1990 December 1-10) and Astro-2 (1995 March 2-18) missions; the images provide an extensive FUV mosaic of the SMC (Cornett et al. 1997) and contain numerous regions in the LMC, covering a wide range of stellar densities and current star formation activity. A total of 47 LMC/Lucke-Hodge (=1970AJ.....75..171L) and 37 SMC/Hodge (=1985PASP...97..530H) OB associations are completely or partially included in the observed fields. FUV data can identify the hottest OB stars more easily than optical photometry can, and these stars dominate the ionizing flux, which is correlated to the observed H-alpha flux of the associated HII regions. Of the HII regions in the DEM catalog (=1976MmRAS..81...89D), the UIT fields completely or partially include 102 DEM regions in the LMC and 74 DEM regions in the SMC. More details on UIT hardware, observations, and data reduction are in Stecher et al. (=1992ApJ...395L...1S and =1997PASP..109..584S).
ASTRO 1/UIT, ASTRO 2/UIT
Star IDs, RA and Dec coordinates, field name, X and Y coordinates, magnitudes and errors ID Running ID number or star, ordered in RA -- RAh Hours of RA coordinate (Epoch 2000.0) h RAm Minutes of RA coordinate min RAs Seconds of RA coordinate Mean uncertainty in UIT positions is approximately 2 arcsec, with smaller values near field centers (X=1023.5, Y=1023.5) and larger values near the edges. The PSF has a FWHM~3.4 arcsec. s DE- Declination sign --- DEd Degrees of Dec coordinate (Epoch 2000.0) deg DEm Minutes of Dec coordinate arcmin DEs Seconds of Dec coordinate arcsec Field Name of UIT field in which the star appears Fields are 37 arcmin in diameter; locations of Fields are shown in the printed paper. --- X X coordinate of star's location in "Field" 1 pix = 1.13 arcsec; images are NOT oriented "north up", so cardinal directions relative to X and Y positions will vary from field to field. These X and Y coordinates are for use in locating objects on the finder charts in the paper; RA and Dec positions should be used for other cases. pix Y Y coordinate of star's location in "Field" pix Mag_B1 Magnitude of star in UIT B1 filter (1521 A) UIT magnitudes are defined by m_lambda = -2.5 log(F_lambda) - 21.1 where F_lambda is in units of ergs/cm^2/Angstrom/s and is the mean flux per Angstrom over the UIT bandpass converted from the measured counts from PSF photometry. The Mag_B1 magnitudes in this table are made with UIT's "B1" bandpass, which has an effective wavelength (for a flat input spectrum) of 1521 Angstroms, a peak at 1443 Angstroms, and an effective width of 354 Angstroms. These magnitudes are termed "m(152)", "m(B1)", and "m_B1" in the literature. mag e_B1 Photometric uncertainty in B1 magnitude This is the uncertainty returned by UITPHOT, an IDL/UIT implementation of DAOPHOT which incorporates the noise characteristics of UIT. It includes sky and other photometric uncertainties, but no absolute calibration uncertainty. From comparison with IUE spectra, the uncertainty in the absolute calibration is about 0.15 for typical stars in this table. mag o_B1 Number of observations to determine B1 mag --- Mag_B5 Magnitude of star in UIT B5 filter (1615 A) UIT magnitudes are defined by m_lambda = -2.5 log(F_lambda) - 21.1 where F_lambda is in units of ergs/cm^2/Angstrom/s and is the mean flux per Angstrom over the UIT bandpass converted from the measured counts from PSF photometry. The Mag_B5 magnitudes in this table are made with UIT's "B5" bandpass, which has an effective wavelength (for a flat input spectrum) of 1615 Angstroms, a peak at 1518 Angstroms, and an effective width of 225 Angstroms. These magnitudes are termed "m(162)", "m(B5)", and "m_B5" in the literature. mag e_B5 Photometric uncertainty in B5 magnitude mag o_B5 Number of observations to determine B5 mag --- Joel Wm. Parker Southwest Research Institute 1998 Jul 30 J_AJ_116_180.xml Ca II H and K photometry on the uvby system. III. The metallicity calibration for the red giants. J/AJ/116/1922 J/AJ/116/1922 CaII H and K filter photometry III. Ca II H and K photometry on the uvby system. III. The metallicity calibration for the red giants. B J Anthony-Twarog B A Twarog Astron. J. 116 1922 1998 1998AJ....116.1922A J/AJ/109/2828 : CaII H and K filter photometry II. (Twarog+ 1995) Anthony-twarog et al., Paper I. 1991AJ....101.1902A Twarog & Anthony-twarog, Paper II. 1995AJ....109.2828T, Cat. <J/AJ/109/2828> Photometry, uvby Stars, population II stars: abundances stars: Population II techniques: photometric New photometry on the uvby Ca system is presented for over 300 stars. When combined with previous data, the sample is used to calibrate the metallicity dependence of the hk index for cooler, evolved stars. The metallicity scale is based upon the standardized merger of spectroscopic abundances from 38 studies since 1983, providing an overlap of 122 evolved stars with the photometric catalog. The hk index produces reliable abundances for stars in the [Fe/H] range from -0.8 to -3.4, losing sensitivity among cooler stars due to saturation effects at higher [Fe/H], as expected.
New CTIO 1 meter photometry Star HD or BD name --- Vmag V magnitude mag b-y b-y colour index mag m1 m_1_ colour index mag c1 c_1_ colour index mag hk hk [(Ca-b) - (b-y)] colour index mag e_Vmag rms uncertainty on Vmag mag e_b-y rms uncertainty on b-y mag e_m1 rms uncertainty on m1 mag e_c1 rms uncertainty on c1 mag e_hk rms uncertainty on hk mag o_Vmag Number of nights on which V, b-y and hk were observed --- o_m1 Number of nights on which m1 and c1 were observed --- Names Other names --- James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_1922.xml Modeling the diversity of outer planetary systems. J/AJ/116/1998 J/AJ/116/1998 Outer planetary systems Modeling the diversity of outer planetary systems. H F Levison J J Lissauer M J Duncan Astron. J. 116 1998 1998 1998AJ....116.1998L Planets Solar system Models, evolutionary celestial mechanics, stellar dynamics solar system: formation solar system: general In order to better understand the range of dynamically long-lived giant planet systems, we present the results of a set of bottom-up numerical simulations designed to generate plausible giant planet systems from a large number of planetary embryos. Our simulations produced systems that are stable for at least a billion years and that exhibit a wide range of characteristics. Some of these systems are reminiscent of the outer solar system. The number of planets ranged from one to seven. Many systems contained only Uranus-mass objects. We constructed systems that were more compact than the outer solar system and systems that were much sparser, with planets on very eccentric orbits. Perhaps most surprisingly, some of the systems that we constructed were stable for at least a billion years despite undergoing macroscopic orbital changes on much shorter timescales.
Orbital elements Run Run number --- f Physical radius of a planet relative to the radius of its Hill sphere flag number=1 a: f=0.1 b: f=7*10^-4^ --- Mass Mass in Earth masses geoMass a Semimajor axis AU e Eccentricity --- i Inclination deg w Argument of perihelion deg W Longitude of the ascending node deg M Mean anomaly deg James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_1998.xml A photometric and kinematic study of AWM 7. J/AJ/116/2108 J/AJ/116/2108 AWM 7 radial velocities A photometric and kinematic study of AWM 7. D M Koranyi M J Geller J J Mohr G Wegner Astron. J. 116 2108 1998 1998AJ....116.2108K J/AJ/109/874 : Kinematics of MKW and AWM Poor Clusters (Beers+ 1995) Clusters, galaxy Magnitudes Radial velocities galaxies: clusters: individual (AWM 7) galaxies: luminosity function, mass function We have measured redshifts and Kron-Cousins R-band magnitudes for a sample of galaxies in the poor cluster AWM 7. We have measured redshifts for 172 galaxies; 106 of these are cluster members. We determine the luminosity function (LF) from a photometric survey of the central 1.2x1.2h^-1^Mpc. The LF has a bump at the bright end and a faint-end slope of {alpha}=-1.37+/-0.16, populated almost exclusively by absorption-line galaxies. The cluster velocity dispersion is lower in the core (~530km/s) than at the outskirts (~680km/s), consistent with the cooling flow seen in the X-ray. The cold core extends ~150h^-1^kpc from the cluster center. The Kron-Cousins R-band mass-to-light ratio of the system is 650+/-170hM_{sun}_/L_{sun}_, substantially lower than previous optical determinations, but consistent with most previous X-ray determinations. We adopt H_0_=100hkm/s/Mpc throughout this paper; at the mean cluster redshift (5247+/-76km/s), 1h^-1^Mpc subtends 65.5'.
Properties of sample galaxies RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declinatin sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec RV Radial velocity km/s e_RV rms uncertainty on RV km/s Rmag Isophotal magnitude (to 23.5mag/arcsec^2^ in R_KC_) mag e_Rmag rms uncertainty on Rmag mag r_Rmag Source of the magnitude (CCD frame number or P for POSS) --- Em Emission type number=1 Ab: absence of H{alpha} Em: emission-line H{alpha} equivalent widths typically >7{AA} --- AR Extinction A_R_ along the line of sight to the galaxy mag James Marcout, Patricia Bauer CDS 1998 Dec 15 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_2108.xml Recent star formation in Sextans A. J/AJ/116/2341 J/AJ/116/2341 UBVRI photometry in Sextans A Recent star formation in Sextans A. S D Van Dyk D Puche T Wong Astron. J. 116 2341 1998 1998AJ....116.2341V Galaxies, nearby Photometry, UBVRI Stars, luminous galaxies: dwarf galaxies: evolution galaxies: individual (Sextans A, DDO 75) galaxies: photometry galaxies: stellar content Local Group We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.
UBV(RI)_c_ photometry of 2525 stars StarID Star identification --- Xpos X Pixel number pix Ypos Y Pixel number pix RAh Right Ascension (2000) h RAm Right Ascension (2000) min RAs Right Ascension (2000) s DE- Declination sign (2000) --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Vmag V magnitude mag e_Vmag Error in V magnitude mag U-B U-B color mag e_U-B Error in U-B color mag B-V B-V color mag e_B-V Error in B-V color mag V-R V-R color mag e_V-R Error in V-R color mag R-I R-I color mag e_R-I Error in R-I color mag Schuyler Van Dyk IPAC 1998 Oct 30 Schuyler Van Dyk <vandyk@ipac.caltech.edu> J_AJ_116_2341.xml WFPC2 observations of star clusters in the Magellanic clouds. II. The oldest star clusters in the Small Magellanic Cloud. J/AJ/116/2395 J/AJ/116/2395 BV photometry in five SMC clusters WFPC2 observations of star clusters in the Magellanic clouds. II. The oldest star clusters in the Small Magellanic Cloud. K J Mighell A Sarajedini R S French Astron. J. 116 2395 1998 1998AJ....116.2395M Clusters, open Magellanic Clouds Photometry, UBV galaxies: evolution galaxies: individual (SMC) galaxies: star clusters Local Group We present our analysis of archival Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) observations in F450W (~B) and F555W (~V) of the intermediate-age populous star clusters NGC 121, NGC 339, NGC 361, NGC 416, and Kron 3 in the Small Magellanic Cloud. We use published photometry of two other SMC populous star clusters, Lindsay 1 and Lindsay 113, to investigate the age sequence of these seven star clusters in order to improve our understanding of the formation chronology of the SMC. We analyzed the V versus B-V and M_V_ versus (B-V)_0_ color-magnitude diagrams of these populous Small Magellanic Cloud star clusters using a variety of techniques and determined their ages, metallicities, and reddenings. These new data enable us to improve the age-metallicity relation of star clusters in the Small Magellanic Cloud. In particular, we find that a closed-box continuous star formation model does not reproduce the age-metallicity relation adequately. However, a theoretical model punctuated by bursts of star formation is in better agreement with the observational data presented herein.
WFPC2 stellar photometry of the SMC clusters NGC 416, 121, 339, 361 and Kron 3 Cluster Cluster name --- MSF Identification number in the cluster number=1 Cl* "Cluster" MSF Nyyyyxxxx in Simbad, where N is the WFPC2 chip number (1, 2, 3 or 4), yyyy the y coordinate of the star multiplied by 10 and xxxx the x coordinate of the star multiplied by 10. --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V colour index mag e_B-V rms uncertainty on B-V mag James Marcout, Patricia Bauer CDS 1999 Jan 05 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_2395.xml Multicolor CCD photometry of the poorly studied globular cluster M80. J/AJ/116/2415 J/AJ/116/2415 CCD UBVRI Photometry of M80 Multicolor CCD photometry of the poorly studied globular cluster M80. G Alcaino W Liller F Alvarado V Kravtsov A Ipatov N N Samus O Smirnov Astron. J. 116 2415 1998 1998AJ....116.2415A Clusters, globular Photometry, CCD Photometry, UBVRI The table photom.dat contains the first multicolour (UVBRI) CCD photometry of 4899 stars in a 4'x7' field of the poorly studied globular cluster M80. The observations were acquired on 1994 June 13-16 using the 2.5m telescope of the Las Campanas Observatory, with a 2x1024x1024 pixel CCD. Two observing 4'x4' fields were observed, the first one at the cluster center, and the second one centered at approximately 3' to the East of the cluster center. The limiting magnitude was deeper in the the second frame by approximately DV=2.5mag. The exposures were 8 to 500s, with a total of 7 frames in U, 17 frames in B, 20 frames in V, and 18 frames in I.
M 80 NGC 6093 C 1614-228 16 17 02.4 -22 58 30
UBVRI in M80 Seq Running number --- xpos Coordinate (along DEC, increases to the south) pix ypos Coordinate (along RA, increases to the east) pix Vmag V magnitude mag U-B U-B color mag B-V B-V color mag V-I V-I color mag Francois Ochsenbein CDS 1999 Jan 20 It is a pleasure to thank Nikolai N. Samus <samus@sai.msu.su> who kindly supplied the data files to CDS. J_AJ_116_2415.xml HW Persei: an eclipsing binary at critical contact? J/AJ/116/2549 J/AJ/116/2549 HW Per UBV differential photometry HW Persei: an eclipsing binary at critical contact? R G Samec B J Carrigan R J McDermith Astron. J. 116 2549 1998 1998AJ....116.2549S Binaries, spectroscopic Photometry, UBV binaries: close binaries: eclipsing stars: variables: other techniques: photometric A complete photometric analysis for the eclipsing binary candidate HW Persei is presented. The UBV observations were taken at Lowell Observatory in 1996 January. Three epochs of minimum light were determined, and an improved linear ephemeris was calculated. The O-C residuals, spanning some 60 years, show no evidence of a period change. Standard magnitudes are given, and reddening estimates are made. The first published synthetic light curve solutions of HW Per reveal that it is near a state of critical contact, which we define as both components exactly filling their respective Roche lobes. The primary component is of A8 spectral type, and the secondary component is a K3-K4 spectral type. The nature of the model is discussed.
HW Per 03 58 42.0 +44 43 18
Standardized observations of HW Persei HJD Heliocentric Julian date d band Filter --- Dmag Differential magnitude in Band filter HW Per - Comparison star number=1 Comparison star: RA=03:58:51, DE=+44:36:37 (J2000.0) mag James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_2549.xml The universality of the fundamental plane of E and S0 galaxies: sample definition and I-band photometric data. J/AJ/116/2728 J/AJ/116/2728 I photometry of early-type galaxies The universality of the fundamental plane of E and S0 galaxies: sample definition and I-band photometric data. M Scodeggio R Giovanelli M P Haynes Astron. J. 116 2728 1998 1998AJ....116.2728S VII/26 : Uppsala General Catalogue of Galaxies (UGC) (Nilson 1973) VII/118 : NGC 2000.0 (Sky Publishing, ed. Sinnott 1988) J/AJ/116/2738 : Spectroscopy of early-type galaxies (Scodeggio+ 1998) Galaxies, photometry Morphology Photometry, CCD Radial velocities Galaxy catalogs Velocity dispersion distance scale galaxies: distances and redshifts galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: photometry As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.
Measured photometric parameters Name Galaxy name number=1 UGC (Cat. <VII/26>) or A (Giovanelli & Haynes private galaxy catalog, AGC, Arecibo General Catalog) designation Individual notes: A111067, UGC 688, A110044, A111068: within the halo of the galaxy UGC 689 A110055: bright companion nearby (UGC 700) UGC 735: faint outer ring --- NGC/IC NGC or IC (Cat. <VII/118>) designation --- CGCG CGCG (Cat. <VII/49>) or Dressler (D, 1980, Cat. <VII/174>) designation --- RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign (B1950.0) --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec MType RC3 (<VII/155>) morphological type code --- HRV Heliocentric radial velocity km/s RadE Measured effective radius arcsec RadEC Effective radius corrected for seeing effects arcsec e_RadE rms uncertainty on effective radius arcsec Rad Corrected metric effective radius kpc SuBrE Measured effective surface brightness in I band mag/arcsec+2 SuBrEC Corrected effective surface brightness in I band mag/arcsec+2 e_SuBrE rms uncertainty on SuBre mag/arcsec+2 Imag Measured apparent I-band magnitude mag ImagC Corrected apparent I-band magnitude mag e_Imag rms uncertainty on Imag mag IMAG Absolute I magnitude mag Q Quality codes number=2 First digit: photometric code: 1: observation obtained in photometric conditions, uncertainty in the zero-point determination less than 0.03mag 2: observation obtained in photometric conditions, uncertainty in the zero-point determination 0.03-0.05mag 6: observation obtained in nonphotometric conditions, uncertainty in the zero-point determination less than 0.03mag 7: observation obtained in nonphotometric conditions, uncertainty in the zero-point determination 0.03-0.06mag Second digit: image quality code: 0: the image is OK 1: a small amount of contamination from nearby stars or other galaxies 2: a significant amount of contamination from nearby stars or other galaxies 3: iterative subtraction of the contaminating object required 4: flat-fielding of substandard quality due to scattered light from a nearby bright star Thrid digit: profile code: 1: r^1/4^ fit good at all radii 2: r^1/4^ fit acceptable at all radii 3: r^1/4^ fit good only in the core of the galaxy 4: r^1/4^ fit does not provide an acceptable description of the observed photometric profile --- James Marcout, Patricia Bauer CDS 1999 Feb 04 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_2728.xml The universality of the fundamental plane of E and S0 galaxies: spectroscopic data. J/AJ/116/2738 J/AJ/116/2738 Spectroscopy of early-type galaxies The universality of the fundamental plane of E and S0 galaxies: spectroscopic data. M Scodeggio R Giovanelli M P Haynes Astron. J. 116 2738 1998 1998AJ....116.2738S VII/26 : Uppsala General Catalogue of Galaxies (UGC) (Nilson 1973) VII/118 : NGC 2000.0 (Sky Publishing, ed. Sinnott 1988) J/AJ/116/2728 : I photometry of early-type galaxies (Scodeggio+, 1998) Galaxy catalogs Radial velocities Velocity dispersion distance scale galaxies: distances and redshifts galaxies: elliptical and lenticular, cD galaxies: fundamental parameters galaxies: kinematics and dynamics We present central velocity dispersion measurements for 325 early-type galaxies in eight clusters and groups of galaxies, including new observations for 212 galaxies. The clusters and groups are the A262, A1367, Coma (A1656), A2634, Cancer, and Pegasus Clusters and the NGC 383 and NGC 507 Groups. The new measurements were derived from medium-dispersion spectra that cover 600{AA} centered on the Mg I b triplet at {lambda}~5175{AA}. Velocity dispersions were measured using the Tonry & Davis (1979AJ.....84.1511T) cross-correlation method, with a typical accuracy of 6%. A detailed comparison with other data sources is made.
Measured spectroscopic parameters Name Galaxy name number=1 UGC (Cat. <VII/26>) or A (Giovanelli & Haynes private galaxy catalog, AGC, Arecibo General Catalog) designation --- NGC/IC NGC or IC (Cat. <VII/118>) designation --- CGCG CGCG (Cat. <VII/49>) or Dressler (D, 1980, Cat. <VII/174>) designation --- RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign (B1950.0) --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec MType Morhological type code in RC3 (Cat. <VII/155>) --- HRV Heliocentric radial velocity km/s sigma Measured stellar velocity dispersion km/s Vrot Measured rotation velocity km/s sigmac Velocity dispersion corrected for galaxy rotation km/s logsigmac logarithm of the rotation-corrected velocity dispersion [km/s] e_logsigmac rms uncertainty on logsigmac [km/s] logsigman logarithm of the aperture-corrected velocity dispersion [km/s] Ref References for other velocity dispersion measurements number=2 1: Faber et al., 1989ApJS...69..763F (Erratum in 1989ApJS...71..173F) 2: Lucey et al., 1991MNRAS.253..584L 3: Dressler, 1987ApJ...317....1D 4: Lucey et al., 1997MNRAS.287..899L --- Spectroscopic parameters from the literature Name Galaxy name number=1 UGC (Cat. <VII/26>) or A (Giovanelli & Haynes private galaxy catalog, AGC, Arecibo General Catalog) designation --- NGC/IC NGC or IC (Cat. <VII/118>) designation --- CGCG CGCG (Cat. <VII/49>) or Dressler (D, 1980, Cat. <VII/174>) designation --- RAh Right ascension (B1950.0) h RAm Right ascension (B1950.0) min RAs Right ascension (B1950.0) s DE- Declination sign (B1950.0) --- DEd Declination (B1950.0) deg DEm Declination (B1950.0) arcmin DEs Declination (B1950.0) arcsec MType Morhological type code in RC3 (Cat. <VII/155>) --- HRV Heliocentric radial velocity km/s sigma Measured stellar velocity dispersion km/s logsigma logarithm of the velocity dispersion [km/s] e_logsigma rms uncertainty on logsigma [km/s] logsigman Aperture-corrected logarithm of the velocity dispersion [km/s] Ref References for other velocity dispersion measurements number=2 1: Faber et al., 1989ApJS...69..763F (Erratum in 1989ApJS...71..173F) 2: Lucey et al., 1991MNRAS.253..584L 3: Dressler, 1987ApJ...317....1D 4: Lucey et al., 1997MNRAS.287..899L --- James Marcout, Patricia Bauer CDS 1999 Feb 04 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_2738.xml Spectroscopy of outlying H II regions in spiral galaxies: abundances and radial gradients. J/AJ/116/2805 J/AJ/116/2805 H II regions in spiral galaxies Spectroscopy of outlying H II regions in spiral galaxies: abundances and radial gradients. L Van Zee J J Salzer M P Haynes A A O'Donoghue T J Balonek Astron. J. 116 2805 1998 1998AJ....116.2805V VII/118 : NGC 2000.0 (Sky Publishing, ed. Sinnott 1988) Abundances Galaxies, optical H II regions galaxies: abundances galaxies: ISM galaxies: spiral We present the results of low-dispersion optical spectroscopy of 186 HII regions spanning a range of radius in 13 spiral galaxies. Abundances for several elements (oxygen, nitrogen, neon, sulfur, and argon) were determined for 185 of the HII regions. As expected, low metallicities were found for the outlying HII regions of these spiral galaxies. Radial abundance gradients were derived for the 11 primary galaxies; similar to results for other spiral galaxies, the derived abundance gradients are typically -0.04 to -0.07dex/kpc.
Galaxy properties NGC/IC NGC or IC (Cat. <VII/118>) galaxy designation --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec MType Morphological type from RC3 (Cat. <VII/155>) --- Dist Distance Mpc BMAG Absolute B magnitude mag i Inclination from the RC3 (Cat. <VII/155>) deg PA Position angle from RC3 (Cat. <VII/155>) deg R25 Isophotal radius from RC3 (Cat. <VII/155>) arcsec Rad Radius arcsec NHII Number of H II regions --- Spectroscopy observing log NGC/IC NGC or IC (Cat. <VII/118>) galaxy designation --- Slit Slit number --- [VSH98] HII region designation in the galaxy (+XXX+YYY) number=1 [VSH98] NGC NNNN +XXX+YYY, [VSH98] IC NNNN +XXX+YYY in Simbad +XXX east-west offset from the galaxy center in arcsec, east positive +YYY north-south offset from the galaxy center in arcsec, north positive --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec PA Position angle deg Run Run identification --- Nexp Number of exposures --- --- --- Tint Integration time s H II region line strengths NGC/IC NGC or IC (Cat. <VII/118>) galaxy designation --- [VSH98] HII region designation in the galaxy (+XXX+YYY) number=1 [VSH98] NGC NNNN +XXX+YYY, [VSH98] IC NNNN +XXX+YYY in Simbad +XXX east-west offset from the galaxy center in arcsec, east positive +YYY north-south offset from the galaxy center in arcsec, north positive --- Slit Slit number --- [OII] Relative [O II]3727+3729 line strength number=2 line strength relative to H{beta} --- e_[OII] rms uncertainty on [OII] --- [NeIII] Relative [Ne III] 3869 line strength number=2 line strength relative to H{beta} --- e_[NeIII] rms uncertainty on [NeIII] --- [OIII] Relative [O III] 4959+5007 line strength number=2 line strength relative to H{beta} --- e_[OIII] rms uncertainty on [OIII] --- n_[OIII] *: only {lambda}5007 detected (sum derived assuming {lambda}5007/{lambda}4959=2.88) --- [OI] Relative [O I] 6300 line strength number=2 line strength relative to H{beta} --- e_[OI] rms uncertainty on [OI] --- [SIII] Relative [S III] 6312 line strength number=2 line strength relative to H{beta} --- e_[SIII] rms uncertainty on [SIII] --- Halpha Relative H{alpha} 6563 line strength number=2 line strength relative to H{beta} --- e_Halpha rms uncertainty on Halpha --- [NII] Relative [N II] 6548+6583 line strength number=2 line strength relative to H{beta} --- e_[NII] rms uncertainty on [NII] --- [SII] Relative [S II] 6717+6731 line strength number=2 line strength relative to H{beta} --- e_[SII] rms uncertainty on [SII] --- [ArIII] Relative [Ar III] 7136 line strength number=2 line strength relative to H{beta} --- e_[ArIII] rms uncertainty on [ArIII] --- cHbeta Reddening coefficient c_H{beta}_ --- e_cHbeta rms uncertainty on cHbeta --- EWHbeta Hbeta equivalent width 0.1nm H II region ratios NGC/IC NGC or IC (Cat. <VII/118>) galaxy designation --- [VSH98] HII region designation in the galaxy number=1 [VSH98] NGC NNNN +XXX+YYY, [VSH98] IC NNNN +XXX+YYY in Simbad +XXX east-west offset from the galaxy center in arcsec, east positive +YYY north-south offset from the galaxy center in arcsec, north positive --- Rad Radius ? Deprojected radius arcsec Slit Slit number --- [OIII] Line ratio [O III]4959,5007/4363 --- e_[OIII] rms uncertainty on [O III] --- [SII] Line ratio [S II]6717/6731 --- e_[SII] rms uncertainty on [S II] --- log([OII]+[OIII]) log([O II]+[O III]) --- e_log([OII]+[OIII]) rms uncertainty on log([OII]+[OIII]) --- log([OIII]/[OII]) log([O III]/[O II]) --- e_log([OIII]/[OII]) rms uncertainty on log([OIII]/[OII]) --- log([NII]/Ha) log([N II]/H{alpha}) --- e_log([NII]/Ha) rms uncertainty on log([NII]/Ha) --- log([NII]/[OII]) log([N II]/[O II]) --- e_log([NII]/[OII]) rms uncertainty on log([NII]/[OII]) --- log([SII]/[OII]) log([S II]/[O II]) --- e_log([SII]/[OII]) rms uncertainty on log([SII]/[OII]) --- H II region abundances NGC/IC NGC or IC (Cat. <VII/118>) galaxy designation --- [VSH98] HII region designation in the galaxy number=1 [VSH98] NGC NNNN +XXX+YYY, [VSH98] IC NNNN +XXX+YYY in Simbad +XXX east-west offset from the galaxy center in arcsec, east positive +YYY north-south offset from the galaxy center in arcsec, north positive --- Rad Deprojected radius arcsec Slit Slit number --- T(O++) Temperature from O++ K e_T(O++) rms uncertainty on T(O++) number=2 For NGC 4395 +088-119, T(O++)=8930^+5790^_-1200_K K 12+log(O/H) 12+log(O/H abundance --- e_12+log(O/H) rms uncertainty on 12+log(O/H) --- log(N/O) log(N/O) abundance ratio --- e_log(N/O) rms uncertainty on log(N/O) --- log(Ne/O) log(Ne/O) abundance ratio --- e_log(Ne/O) rms uncertainty on log(Ne/O) --- log(S/O) log(S/O) abundance ratio --- e_log(S/O) rms uncertainty on log(S/O) --- log(Ar/O) log(Ar/O) abundance ratio --- e_log(Ar/O) rms uncertainty on log(Ar/O) --- O/Hzkh Zaritsky et al. (1994ApJ...420...87Z) (O/H) abundance ratio --- O/Hep84 Edmunds & Pagel (1984MNRAS.211..507E) (O/H) abundance ratio --- Radial oxygen abundance gradients NGC NGC (Cat. <VII/118>) galaxy designation --- NHII Number of HII regions --- 12+log(O/H) Central 12+log(O/H) abundance --- e_12+log(O/H) rms uncertainty on 12+log(O/H) --- Gradient1 Gradient in dex/r_25_ --- e_Gradient1 rms uncertainty on Gradient1 --- Gradient2 Gradient in dex/r_d_ --- e_Gradient2 rms uncertainty on Gradient2 --- Gradient3 Gradient in dex/kpc --- e_Gradient3 rms uncertainty on Gradient3 --- James Marcout, Patricia Bauer CDS 1999 Feb 04 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_2805.xml A study of nine high-redshift clusters of galaxies. III. Hubble space telescope morphology of clusters 0023+0423 and 1604+4304. J/AJ/116/584 J/AJ/116/584 Cl J0023+0423 and Cl J1604+4304 morphology A study of nine high-redshift clusters of galaxies. III. Hubble space telescope morphology of clusters 0023+0423 and 1604+4304. L M Lubin M Postman J B Oke K U Ratnatunga J E Gunn J G Hoessel D P Schneider Astron. J. 116 584 1998 1998AJ....116..584L J/AJ/116/560 : Cl J0023+0423 and Cl J1604+4304 spectroscopy (Postman+ 1998) http://archive.stsci.edu/mds/mds.cgi : HST Medium Deep Survey WFPC2 catalogOke et al., Paper I. 1998AJ....116..549O Postman et al., Paper II. 1998AJ....116..560P, Cat. <J/AJ/116/560> Clusters, galaxy Morphology Photometry, UBVRI Redshifts cosmology: observations galaxies: clusters: general Galaxy: evolution We present a detailed morphological analysis of the galaxy populations in the first two clusters to be completed in an extensive observational study of nine high-redshift clusters of galaxies. These two clusters, Cl 0023+0423 and Cl 1604+4304, are at redshifts of z=0.84 and z=0.90, respectively. The morphological studies are based on high angular resolution imagery taken with Wide Field Planetary Camera 2 aboard the Hubble Space Telescope. These data are combined with deep, ground-based BVRI photometry and spectra taken with the Keck 10m telescopes. The morphological classifications presented in this paper consist of two parts. First, we provide a quantitative description of the structural properties of ~600 galaxies per cluster field using the Medium Deep Survey automated data reduction and object classification software. This analysis includes the galaxy position, photometry, and best-fit bulge+disk model. Second, for the brightest subsample of ~200 galaxies per cluster field, we provide a more detailed morphological description through a visual classification based on the revised Hubble classification scheme.
GHO 002118+040630 Cl J0023+0423 00 23 52. +04 23 06 GHO 160244+431254 Cl J1604+4303 16 04 25.2 +43 04 52
Cl J0023+0423 field MDS parameters from the automated galaxy classifications Cl J1604+4304 field MDS parameters from the automated galaxy classifications [OPL98] MDS identification number Original identification number from the MDS reduction pipeline. Those numbers that are excluded indicate detected objects that were classified as stars or which did not reach the required signal-to-noise ratio. [OPL98] MDS J0023+0423 NNN in Simbad for table1a.dat [OPL98] MDS J1604+4304 NNN in Simbad for table1b.dat --- Nmod Model number MDS model number: 1, disk; 2, bulge; 3, disk+bulge --- Ntot Total number of pixels in selected region Ntot is the total number of usable pixels in the selected 64 or 128 pixel square region around each object; Npix is the number of Ntot pixels that are more than 1{sigma} above the estimated sky background. --- Npix Total number of pixels in selected region above 1{sigma} --- Nfit Number of parameters in MLE model The number of parameters in the fit that actually vary. A maximum of 12 parameters are fit, though in most cases one or more parameters are held fixed. --- Chip WFPC2 CCD number CCD chip number: PC=1; WFC=2,3,4 --- Xpos X position of centroid of MLE model The mean error between the model centroid and the actual centroid of the object image is 0.2 pixels. Coordinates are relative to each individual chip. pix Ypos Y position of centroid of MLE model pix Sky MLE model Sky magnitude A maximum likelihood estimate for the local sky background is determined simultaneously with the other model parameters. Sufficient pixels are used to ensure that the sky level is determined to an accuracy of 0.5%. The sky background is assumed to be flat over the small region selected for analysis. mag mtot Total MLE model magnitude Small differences between the analytic total magnitude and the true total magnitude may arise because the true galaxy is not smooth, and the model may not average properly over bright regions of star formation. mag e_mtot rms uncertainty on mtot mag logR1/2 Logarithmic half-light radius of MLE model The radius within which half of the light of the unconvolved model would be contained if it were radially symmetric (an axis ratio of unity). Lower and upper limits of 0.1 pixel and one-half of the maximum radius of the region selected for analysis have been imposed. The half-light radius of the individual components can be derived used the bulge/disk half-radius ratio. [arcsec] e_logR1/2 rms uncertainty on logR1/2 [arcsec] P.A. Orientation of MLE model The adopted position angle (measured east from north) is that of the axis of symmetry of the model. It is set equal to zero when the source is assumed to be azimuthally symmetric with an axis ratio of unity. For disk+bulge models, the orientation is assumed to be the same for both components. rad e_P.A. rms uncertainty on P.A. rad b/aD Disk axis ratio of MLE model The ratio of the minor axis half-light ratio to that of the major axis. For disk+bulge models it is defined independently for each component. If the axis is not significantly different from unity, it is fixed at 1. A ratio of zero indicates that this component was not fitted to the data. --- e_b/aD rms uncertainty on e_b/aD --- b/aB Bulge axis ratio of MLE model --- e_b/aB rms uncertainty on e_b/aB --- B/(B+D) Bulge-to-(disk+bulge) luminosity ratio The luminosity of the individual component can be derived from this parameter and the total magnitude mtot. --- e_B/(B+D) rms uncertainty on B/(B+D) --- log(B/D)R1/2 log ratio of bulge/disk half-light radius of MLE model --- e_log(B/D)R1/2 rms uncertainty on (B/D)R1/2 --- SNRIL log integrated signal-to-noise ratio --- Class Name of MLE classification Object classification: object, galaxy, disk, bulge or disk+bulge. --- Asymm Asymmetry parameter --- Cl J0023+0423 field visually classified galaxies Cl J1604+4304 field visually classified galaxies [OPL98] MDS object identifier [OPL98] MDS J0023+0423 NNN in Simbad for table2a.dat [OPL98] MDS J1604+4304 NNN in Simbad for table2b.dat --- mtot Analytic total magnitude Total magnitude of best-fit analytic model in either R_702_ (Cl 0023+0423) or I_814_ (Cl 1604+4304) as given in table 1. mag Class Hubble class The standard Hubble classification scheme (e.g. E, S0, Sa, Sab, Sb) with the addition of the following: E/S0 or S0/E, cannot distinguish between E or S0; X, compact object (likely nonstellar, but too compact to see structure); , peculiar or unclassifiable. --- D Disturbance index 0, normal; 1, moderate asymmetry; 2, strong asymmetric; 3, moderate distortion; 4, strong distortion. --- n_D Interpretation of the disturbance M, merger; I, tidal interaction with neighbor; T, tidal feature; C, chaotic. --- Comm Description of object morphology Here, comp. is short for "companion"; @ indicates position relative to the galaxy going clockwise, e.g. @7 = "at 7 o'clock". --- Cl J0023+0423 field photometry of the visually classified galaxies Cl J1604+4304 field photometry of the visually classified galaxies [OPL98] MDS identification number [OPL98] MDS J0023+0423 NNN in Simbad for table4a.dat [OPL98] MDS J1604+4304 NNN in Simbad for table4b.dat --- Keck Keck Number Corresponding number from the Keck photometry tables (see Paper II, Cat. <J/AJ/116/560>). Because of the better resolution of the HST observations, an individual galaxy in the Keck image may be associated with more than one galaxy in the corresponding HST image. Therefore, these HST galaxies have the same Keck number. --- Bmag B magnitude Keck BVRI aperture photometry. A value of -1.00 indicates no detection in that band mag Vmag V magnitude mag Rmag R magnitude mag Imag I magnitude mag z Redshift --- l_Age limit flag on Age --- Age Galaxy age Galaxy age determined from a comparison between the {tau}=0.6Gyr Bruzual & Charlot (1993ApJ...405..538B) population synthesis model and the broadband AB magnitudes derived from the Keck photometry. Upper limits are indicated as values with no errors. Gyr e_Age rms uncertainty on Age Gyr James Marcout, Patricia Bauer CDS 1998 Nov 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_584.xml An ultraviolet spectral atlas of 10 Lacertae obtained with the Goddard high resolution spectrograph on the Hubble Space Telescope. J/AJ/116/941 J/AJ/116/941 10 Lac UV spectral atlas An ultraviolet spectral atlas of 10 Lacertae obtained with the Goddard high resolution spectrograph on the Hubble Space Telescope. J C Brandt S R Heap E A Beaver A Boggess K G Carpenter D C Ebbets J B Hutchings M Jura D S Leckrone J L Linsky S P Maran B D Savage A M Smith L M Trafton F M Walter R J Weymann M Snow T B Ake R H Hogen Astron. J. 116 941 1998 1998AJ....116..941B J/ApJS/93/211 : IUE survey of H I Ly{alpha} absorption. I. (Diplas+ 1994) Spectra, ultraviolet Stars, O atlases stars: early-type stars: individual (10 Lac) Observations of the narrow-lined O-type star 10 Lacertae taken with the Goddard High Resolution Spectrograph in 1992 November are presented. The spectra cover the wavelength range 1181-1777{AA} with a resolution of 15km/s and signal-to-noise ratio greater than 100:1. Absorption lines arising in the interstellar medium, the photosphere, and the stellar wind are identified and discussed.
HST HD 214680 10 Lac 22 39 15.7 +39 03 01
Interstellar absorption lines detected in the spectrum of 10 Lacertae LambLab Laboratory wavelength 0.1nm LamObs Observed Wavelength 0.1nm Species Species number=1 A single asterisk denotes an excited state, a double asterisk denotes a highly excited state --- HV Heliocentric velocity km/s Note Notes number=2 1: Line appears to be present, identified species is probably the dominant contributor to the observed absorption, blends are definite or likely. 2: Blend with C I {lambda}1188.883. 3: Line is definitely present, sharp and well resolved from neighboring lines; core is not saturated, no known or serious blends, wavelength and velocity appear consistent with other lines 4: Line is definitely present, core is saturated, wings are broader than unsaturated lines, wavelength and velocity appear consistent with other lines. 5: Saturated over 5{AA}. 6: Deep, nearly saturated. 7: Weak but real absorption feature is present at the expected wavelength. 8: Absorption is present in a complex stellar profile; photospheric or narrow absorption component contributions are possible. 9: Badly blended. -- Table of identified lines LamLab Laboratory wavelength 0.1nm LamObs Observed wavelength 0.1nm Com Comments --- James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From AJ electronic version J_AJ_116_941.xml Flux densities, positions, and structures for a complete sample of intense radio sources at 1400MHz. J/AJ/77/405 J/AJ/77/405 Intense radio sources at 1400MHz [BDFL sample] Flux densities, positions, and structures for a complete sample of intense radio sources at 1400MHz. A H Bridle M M Davis E B Fomalont J Lequeux Astron. J. 77 405 1972 1972AJ.....77..405B Radio lines Radio sources Surveys Accurate flux densities, precise positions of unresolved sources, and structures of resolved sources have been derived from full-beam and interferometric observations of intense sources at 1400 MHz. Results are given for 424 sources in the area of sky -5{deg}<{delta}<+70{deg}, |b|>5 whose 1400-MHz integrated flux densities S_1400_ exceed 1.70Jy [1 Jy (flux unit) = 10^-26^w/m^2^/Hz]. The 234 sources with S_1400_>=2.00Jy, equivalent diameters <10arcmin, and |b|>20{deg} form a 98+/-2% complete sample comparable in number to the 178-MHz Revised Third Cambridge Catalogue in this 4.30-sr area of sky, but selected at 1400MHz. This sample is suitable for statistical studies of the properties of extragalactic radio sources. To facilitate its use, and that of other samples which may be drawn from these data, references to other studies of the positions, fine and extended structure, polarization, and variability of the sources have been assembled in the principal table of this paper (Table 2). A comparison is made with other 1400-MHz flux-density data (Sec. 3), and the spectral content of the complete sample is discussed (Sec. 4).
A complete catalogue of intense sources at 1400MHz Source Source designation --- n_Source Note on source number=1 *: sources for which contour maps are given in Fig. 5 +: there is a nearby weak source within a radius of about 20arcmin The flux density, separation, and position angle (defined from the catalogued source towards the weaker source) are given in a footnote, and a more detailed listing is given in table3. #: source which is composed of two widely separated components and which is likely to be an accidental, rather than physical, double --- Name Common source name. LS indicates a lobe shift in the original survey --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s n_RAs Note detailed in file notes.dat --- e_RAs rms uncertainty on right ascension (1950.0) s r_RAh Reference for the right ascension --- DE- Declination sign (1950.0) --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec n_DEs Note detailed in file notes.dat --- e_DEs rms uncertainty on declination (1950.0) arcsec r_DEd Reference for the declination number=2 N, C & KPW: references to data presented in table2.dat 1-6: Polarization data A: Accurate positions for unresolved sources M: Accurate positions and structures and/or maps of extended sources P: Positions only, structures unknown in these measurements S: Structures only VLB: Long baseline interferometry SC: Interplanetary scintillation data VAR: Variable Radio sources All the references are in file "refs.dat" --- GLAT Galactic latitude truncated to nearest degree deg S1400MHz Flux density and standard error at 1400 MHz Jy n_S1400MHz Note detailed in file notes.dat --- e_S1400MHz rms uncertainty on S1400MHz Jy r_S1400MHz Reference for the flux density number=2 N, C & KPW: references to data presented in table2.dat 1-6: Polarization data A: Accurate positions for unresolved sources M: Accurate positions and structures and/or maps of extended sources P: Positions only, structures unknown in these measurements S: Structures only VLB: Long baseline interferometry SC: Interplanetary scintillation data VAR: Variable Radio sources All the references are in file "refs.dat" --- Class Structure type number=3 D: double, T: triple, H: core-halo, C: complex --- n_Class Note detailed in file notes.dat --- l_EW Limit flag on EW --- EW East-west extent arcmin n_EW Note detailed in file notes.dat --- r_EW Reference for east-west extent number=2 N, C & KPW: references to data presented in table2.dat 1-6: Polarization data A: Accurate positions for unresolved sources M: Accurate positions and structures and/or maps of extended sources P: Positions only, structures unknown in these measurements S: Structures only VLB: Long baseline interferometry SC: Interplanetary scintillation data VAR: Variable Radio sources All the references are in file "refs.dat" --- l_NS Limit flag on NS --- NS North-south extent arcmin n_NS Note on NS detailed in file notes.dat --- r_NS Reference for north-south extent number=2 N, C & KPW: references to data presented in table2.dat 1-6: Polarization data A: Accurate positions for unresolved sources M: Accurate positions and structures and/or maps of extended sources P: Positions only, structures unknown in these measurements S: Structures only VLB: Long baseline interferometry SC: Interplanetary scintillation data VAR: Variable Radio sources All the references are in file "refs.dat" --- BClass Brightness classification number=4 H: high brightness, L: low brightness See Bridle el al. (1972, Nature Phys. Sci. 235, 123) This classification is given only for those sources in the complete sample:-5{deg}<DE<70{deg}, angular extent <10' with S>=2.00Jy for |b|>=20{deg} (234 sources) or S>6.00Jy for 5{deg}<=|b|<20{deg} (18 sources) --- n_BClass Note detailed in file notes.dat --- l_P1400MHz Limit flag on P1400MHz --- P1400MHz Integrated degree of polarization at 1400MHz % n_P1400MHz Note detailed in file notes.dat --- PA Position angle of electric vector at 1400MHz deg r_P1400MHz Reference for polarization number=2 N, C & KPW: references to data presented in table2.dat 1-6: Polarization data A: Accurate positions for unresolved sources M: Accurate positions and structures and/or maps of extended sources P: Positions only, structures unknown in these measurements S: Structures only VLB: Long baseline interferometry SC: Interplanetary scintillation data VAR: Variable Radio sources All the references are in file "refs.dat" --- Notes Other references to information concerning the source. For sources resolved by the 300-ft observations, peak flux densities are given in this column --- Individual notes to table2.dat and table4.dat Source Source designation --- Note Text of the note --- Confusing sources Name Catalogue source --- NSource Nearby source --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s n_RAh *: Data from CIT observations --- DE- Declination sign (1950.0) --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec n_DEd *: Data from CIT observations --- GLAT Galactic latitude deg S1400MHz Integrated flux density Jy n_S1400MHz *: Data from CIT observations --- S1400MHzp Peak flux density Jy Sep Separation arcmin PA Position angle from the catalogue source towards the nearby source deg New east-west interferometric observations of resolved sources Source Source designation --- m_Source Multiplicity index on Source number=1 When no multiplicity index, source centroid --- S1400MHz Flux density Jy e_S1400MHz rms uncertainty on S1400MHz Jy l_EW Limit flag on EW --- EW East-West diameter arcmin e_EW rms uncertainty on EW arcmin Pos Position with respect to the source centroid arcmin RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s e_RAs rms uncertainty on right ascension s Note Notes number=2 1: The model fit of the interferometer data is fair. Structure may be more complex. See individual notes in file notes.dat. --- Sources with S_1400_>1.7Jy in other surveys rejected from the present catalogue Survey Survey name --- S Survey flux density Jy n_S (1) --- l_S1400MHz NRAO flux density --- S1400MHz Flux density Jy e_S1400MHz rms uncertainty on S1400MHz Jy RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign (1950.0) --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec u_DEs Uncertainty flag on position --- Notes Notes number=2 1: No identifiable discrete source in field mapped at NRAO 2: Data from Pauliny-Toth et al. (1966ApJS...13...65P) 3: Companion <0.2 Jy within 15' of source 4: Noted in DA as confused with another source 5: Probably confused in original observations by extended background feature I: Scheer and Kraus, 1967AJ.....72..536S II: Dixon and Kraus, 1968AJ.....73..381D III: Fitch et al., 1969AJ.....74..612F IV: Ehman et al., 1970AJ.....75..351E V: Dixon, 1970ApJS...20....1D, Cat. <VII/2> --- Com Comments --- References to table2.dat Ref References designation --- Text Reference --- J. Marcout, P. Bauer CDS H. Andernach Guanajuato Univ. 1999 Jan 29 UNKNOWN UNKNOWN Prepared via OCR at CDS, and proof-read by Heinz Andernach <heinz@astro.ugto.mx> A typo in original paper (note about 0330+16) was corrected to 0300+16 here in file "notes.dat" Some names were corrected in table2.dat on 11-Feb-1999 UNKNOWN UNKNOWN This list if intense radio sources later become known in the astronomical literature as the BDFL sample. J_AJ_77_405.xml The NRAO 5-GHz radio source survey. III. The 140-ft "strong" source survey. J/AJ/77/797 J/AJ/77/797 NRAO 5GHz Strong Source Survey The NRAO 5-GHz radio source survey. III. The 140-ft "strong" source survey. I I K Pauliny-Toth K I Kellermann Astron. J. 77 797 1972 1972AJ.....77..797P VIII/38 : The Parkes-MIT-NRAO 4.85GHz (PMN) Surveys (Griffith+ 1993-1996) J/ApJS/90/173 : PMN map catalog of radiosources (Gregory+, 1994) Davies, Paper I. 1971AJ.....76..980D Pauliny-Toth et al., Paper II. 1972AJ.....77..265P (S1,S2 surveys) Radio sources Surveys The 140-ft telescope at the National Radio Astronomy Observatory has been used to extend the 5-GHz strong source (S) survey over an area of 1.14 steradian. Some 240 sources have been detected in this region, of which 135 are above the completeness limit of 0.6f.u. The distribution of spectral indices for sources above the completeness limit is much broader than for samples selected from long-wavelength surveys, owing to an increase in the fraction of compact sources with flat spectra. For about half of the sources selected at 6 cm, the spectral index {alpha}>-0.5. Analysis of the dependence of the spectral index on the flux density shows that, as expected from the 408-MHz number counts and spectral index distribution, at 5 GHz there are fewer flat spectra among the weak sources than among the stronger ones. The spectral index distributions for the identified galaxies and quasars show the familiar forms: the galaxies have a strong concentration near {alpha}=-0.8 with a small tail extending toward flat spectra. The quasars show a much broader distribution of indices, but the fraction (80%) of quasars having flat spectra ({alpha}>-0.5) is much greater than that found in the low-frequency surveys. The number-flux density relation for various groups of sources selected from the 5-GHz survey show that the anomalously steep slope is confined to (a) unidentified sources, (b) sources with steep spectra ({alpha}<-0.5), and (c) sources located in the north galactic hemisphere. Sources identified with radio galaxies or quasars, or which have flat spectra, or which are in the south galactic hemisphere all show a number-flux density slope near -1.5.
Green Bank 5-GHz strong source survey S3 Object designation --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec n_RAh Origin of the position number=1 blank = position measured with the 140-ft telescope at 5 GHz. OPT= optical position from literature. NRI= position measured with the NRAO interferometer at 2.7 GHz (Clark and Hogg, 1966ApJ...145...21C; Hogg, 1969ApJ...155.1099H; Wade, 1970ApJ...162..381W; Wade and Miley, 1971AJ.....76..101W). RRE= position measured with the interferometer of the Royal Radar establishment, Malvern at 2.7 GHz (Adgie, Crowther, and Gent, 1972MNRAS.159..233A). CAM= position measured with the Cambridge 1-mile synthesis instrument at 1.4 GHz (Parker, Elsmore, and Shakeshaft, 1966Natur.210...22P MacDonald, Kenderdine, and Neville, 1968MNRAS.138..259M; Mackay, 1969MNRAS.145...31M; Elsmore and Mackay, 1969MNRAS.146..361E). PKT= Parkes transit measurements at 2.7 GHz (Shimmins, Clarke, and Ekers, 1966AuJPh..19..649S). CT21= position measured with OVRO interferometer at 1.4 GHz (Fomalont and Moffet, 1971AJ.....76....5F). BOL= position from Bologna surveys at 408 MHz (Grueff and Vigotti, 1968ApL.....2..113G; Colla et al., 1970, Cat. <VIII/36>, 1972, Cat. <VIII/36>). 300= position measured with the 300-ft telescope at 1.4 GHz (Pauliny-Toth, Wade, and Heeschen, 1966ApJS...13...65P). --- S5GHz Flux density at 5GHz Jy n_SI > when lower limit --- SI Spectral index below 5GHz number=2 The spectral index is defined here as flux {prop.to} {nu}^{alpha}^ --- e_SI rms uncertainty on SI --- Ident Optical identification number=4 QSS: quasars with spectroscopic or photometric confirmation GAL: galaxy of undetermined type E: elliptical galaxy D: D galaxy DB: dumbbell galaxy SEY: Seyfert galaxy N: N galaxy EF: empty field (no object above plate limit or neutral star) CF: confused field: several galaxies or stellar objects in field --- n_Ident : tentative identification number=3 An asterisk denotes a tentative identification, e.g., a suggested QSS with no photometric or spectroscopic confirmation. Identifications made on the basis of the present work are indicated by a reference to a footnote in column Notes which also gives the origin of the position used others are taken from the literature. Identification are only given for sources above the completeness limit --- Notes Individual notes detailed in file "notes.dat" --- Cat Membership in other catalogs --- Notes on table2.dat NoteID Note number, repeated when several lines are needed. --- Text Text of note --- James Marcout, Patricia Bauer CDS 1998 Oct 20 UNKNOWN UNKNOWN Prepared via OCR at CDS, and proof-read by Heinz Andernach (heinz@astro.ugto.mx). J_AJ_77_797.xml Classification of 831 two-micron sky survey sources south of +5deg J/AJ/80/1011 J/AJ/80/1011 IRC classification Classification of 831 two-micron sky survey sources south of +5deg O L Hansen V M Blanco Astron. J. 80 1011 1975 1975AJ.....80.1011H Plate data Stars, carbon Stars, S Surveys Eight hundred thirty-one infrared sources located south of +5deg have been selected from the Two-Micron Sky Survey (IRC), and studied in an objective-prism survey. The set consists of all 551 sources which were not identified in the IRC, 97 source whose identification in the IRC is questionable, and 183 sources identified by their variable-star catalog name, but for which no classification is given in the IRC. The great majority (89%) of the sources studied are M stars, but 49 carbon stars and seven S stars as well as 17 peculiar stars with emission near 8600A have also been identified. If available, recent classifications or identifications from other investigators are included
Classification of southern IRC sources IRC IRC number --- Kmag K magnitude mag I-K I-K colour mag Vmag V magnitude mag Type IRC classification --- Var Star name of those variable stars included in the program for their lack of classification --- Sp Spectral type --- Bright Relative brightness number=1 Subjective estimate of the source brightness as it appears in the 10-min-exposure plates. vb: very bright b: bright mb: medium bright mf: medium faint f: faint vf: very faint t: trace nt: no trace --- com Comments --- Marie-Jose Wagner, Patricia Bauer CDS 1994 Dec 05 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_80_1011.xml A study of the motion, membership, and distance of the Hyades cluster J/AJ/80/379 J/AJ/80/379 Hyades cluster: motion, membership, and distance A study of the motion, membership, and distance of the Hyades cluster R B Hanson Astron. J. 80 379 1975 1975AJ.....80..379H Photometry, photographic Plate data Proper motions Stars, faint New absolute proper motions referred directly to external galaxies, photographic photometry, and cluster membership probabilities have been determined for over 600 faint stars in the Hyades region. These have been used to investigate the Hyades convergent point and distance. A detailed review of the foundations of the convergent-point method, its applicability to the Hyades, the several mathematical variations of the method, and its possible role in producing the apparent discrepancy between previous Hyades proper motion results and "secondary" Hyades distance indicators, has been carried out. The convergent-point method, as applied to the Hyades, is entirely valid, and cannot be the source of any significant error in the Hyades distance. Systematic errors in meridian circle proper motions are implicated as the cause of the observed Hyades distance discrepancy. The convergent-point analysis of the new absolute Hyades proper motions represents the first Hyades distance determination independent of all meridian circle proper motion systems. The resulting Hyades distance modulus is m-M = 3.42, significantly greater than all previous values from proper motions, and in agreement with predictions of the Hyades distance from stellar structure theory, and with the results of "secondary" distance indicators. Incorporating this value, the most likely value of the mean Hyades distance modulus from all sources is m-M = 3.29+/-0.08. The quoted error represents a larger and more realistic estimate of the true errors than has been previously stated. Significant effects of the increased Hyades distance on the cosmic distance scale and other questions of general astronomical importance are briefly discussed.
Identification, positions, magnitudes, proper motions, and Hyades membership probabilities Star Star number --- VA Van Altena (1966,1969) number --- Luyten Luyten (1971) designation --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vmag V magnitude mag B-V B-V colour index mag Type Star type number=1 2=faint reference star 3=AGK 2 catalogue star 4=photoelectric photometry star 5=selected on blink survey --- SystCode System code number=2 1=long exposure 2=short exposure 3=both exposures --- Measur Number of images measured at each epoch --- pmRA Proper motion in right ascension arcsec/yr pmDE Proper motion in declination arcsec/yr e_pmRA Error on proper motion in RA mas/yr e_pmDE Error on proper motion in DE mas/yr MembProb Hyades cluster membership probability % Note Note number=3 1. No yellow plate measures exist for these stars. Approximate B magnitudes are: No 34 332 395 404 406 575 ---------------------------------------------- Bmag 18.04 13.40 18.57 18.12 18.72 17.87 2. Image interference on blue plates with nearby bright star. (B-V) suspect. 3. Near plate edge. (B-V) suspect. 4. Severe image interference on plates. No. 350: Only first-epoch position measurable. No. 616: OS 996, near {alpha} Tau, all data may be suspect. Bmag~11.9. --- Marie-Jose Wagner, Simona Mei CDS 1995 Aug 30 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_80_379.xml 5-GHz survey of bright galaxies. J/AJ/80/771 J/AJ/80/771 5-GHz Survey of Bright Galaxies 5-GHz survey of bright galaxies. R Sramek Astron. J. 80 771 1975 1975AJ.....80..771S VII/16 : Reference Cat. of Bright Galaxies (1st Ed.) (de Vaucouleurs+ 1964) VII/112 : RC2 Catalogue (de Vaucouleurs+ 1976) VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991) Galaxy catalogs Radio continuum The 1135 galaxies in the Reference Catalogue of Bright Galaxies (Cat. <VII/16>) with declinations between +10{deg} and +70{deg} were surveyed at 6-cm wavelength with a 3-sigma detection limit of about 30mf.u.; of these 149 were detected. For 90 of these galaxies, spectral indices were obtained. There is a suggestion that the elliptical galaxies have flat spectra more often than the spiral galaxies.
Galaxy flux densities Galaxy Galaxy name number=1 N prefix denotes an NGC (See Cat. <VII/118/>) galaxy, I is an IC (See Cat. <VII/118/>) galaxy, an A an anonymous galaxy. --- l_F5GHz lower limit flag --- F5GHz Final flux density at 5GHz mJy e_F5GHz rms uncertainty on F5GHz mJy n_F5GHz Notes on F5GHz number=2 P: possible detection; the flux density measured with the 300ft was less than twice the error of the 140ft flux and, therefore, the detection was considered unconfirmed PC: this is only a possible detection since there was a confusing source nearby R: the flux measured with the 140ft was greater than 1.6 times the flux from the 300ft and the difference exceeds the range of the errors of the two measurements. These sources are probably resolved with the 300ft beam or they have a complex structure. The flux density given is the 140ft measurement and the errors may be larger than indicated. O: the source is offset from the galaxy position. The amount and direction of this offset is mentioned in the Notes column. --- Note N: note detailed in file "notes.dat" --- Diam Note on the diameter number=3 D: the optical diameter from the RCBG (Cat. <VII/16/>) is greater than 6 arcmin; the radio source is not necessarily resolved, but the flux densities of these large galaxies should be used with caution. --- l_SI Limit flag on SI --- SI Spectral index of the source number=4 The spectral index is defined here as flux ~ {nu}^{alpha} --- Ref References for a second flux-density measurement number=5 References for flux densities used in determining the spectral indices A: Dwingeloo Survey (Dixon, 1970, Cat. <VII/2>) B: Ohio Survey (Dixon, 1970, Cat. <VII/2>) C: De Jong (1967ApJ...150....1D) D: De La Beaujardiere et al. (1968AnAp...31..387D) E: Lang and Terzian (1969ApL.....3...29L) F: Bologna Survey-B2 (Dixon, 1970, Cat. <VII/2>) G: Cambridge Survey-5C2 (Dixon, 1970, Cat. <VII/2>) H: Cameron (1971MNRAS.152..403C) I: Kellermann et al. (1969ApJ...157....1K) J: Cambridge Survey-5C4 (Willson, 1970MNRAS.151....1W) K: Rogstad et al. (1973A&A....22..111R) L: van der Kruit (1973A&A....29..231V) M: Tovmassian and Terzian (1974PASP...86..649T) All spectral indices without references are based on the 1410-MHz observations of Pfleiderer (1972MitAG..31....1P) --- Notes Offset position and notes when n_F5GHz = "O " --- Individual notes Galaxy Galaxy name --- Note Text of the note --- James Marcout, Patricia Bauer CDS 1998 Oct 20 UNKNOWN UNKNOWN Prepared via OCR at CDS, and proof-read by Heinz Andernach (heinz@astro.ugto.mx). J_AJ_80_771.xml A study of field galaxies. I. Redshifts and photometry of a complete sample of galaxies J/AJ/83/1549 J/AJ/83/1549 A study of field galaxies. I. A study of field galaxies. I. Redshifts and photometry of a complete sample of galaxies R P Kirshner A Oemler Jr. P L Schechter Astron. J. 83 1549 1978 1978AJ.....83.1549K J/AJ/88/1285 : A deep survey of galaxies (Kirshner+ 1983) J/AJ/95/1629 : [O III] emission in 2 field-galaxy surveys (Moody+ 1988) Galaxies, photometry Redshifts As a first step towards a redetermination of the luminosity function and space distribution of field galaxies, we present data on a magnitude limited sample of galaxies in eight fields in the north and south galactic polar caps. Redshifts, accurate to about 100 km/s have been obtained for 164 of 184 galaxies brighter than J=15.0 (B~15.5) We have also measured magnitudes and colors for a large sample of 807 galaxies, complete to J~15.7.
Galaxy photometry results Field Field designation --- Galaxy Galaxy name --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec SpType Spectral type --- Jmag J magnitude number=1 When the photographic photometry was bad, the magnitude is estimated to 0.1mag and no color is given. In NP6, our red plate was too small to cover the entire region surveyed in J. Galaxies without colors are those beyond the red field. mag J-F J-F colour index number=1 When the photographic photometry was bad, the magnitude is estimated to 0.1mag and no color is given. In NP6, our red plate was too small to cover the entire region surveyed in J. Galaxies without colors are those beyond the red field. mag Vel Velocity km/s n_Vel Indication on rms velocity uncertainty number=2 The rms uncertainty on the velocities, as determined from the scatter in velocity determinations from individual lines is 100km/s. Velocities that have internal accuracies at least a factor of 2 better than the mean are indicated by a "+" sign, those that are a factor of 2 worse than the mean are indicated by a "-" sign. --- Com Comments number=3 BGM/BCM: Brightest group/cluster member CR: Chincarini and Rood (1972AJ.....77....4C) DGH: Davis, Geller, and Huchra (1978ApJ...221....1D) SRC: Second Reference Catalogue (De Vaucouleurs et al. 1976) Cat. <VII/112> GT: Gregory and Thompson (1978ApJ...222..784G) --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_83_1549.xml Complete samples of active extragalactic objects. II. A deep 1.452-GHz VLA survey centered on 08:52:15+17:16 J/AJ/87/1429 J/AJ/87/1429 Active extragalactic objects II. Complete samples of active extragalactic objects. II. A deep 1.452-GHz VLA survey centered on 08:52:15+17:16 J J Condon K J Mitchell Astron. J. 87 1429 1982 1982AJ.....87.1429C J/AJ/87/739 : Active Extragalactic Objects I. (Condon+ 1982) J/AJ/90/1437 : Active Extragalactic Objects III (Coleman+ 1985) Radio sources A single primary-beam area centered on alpha=08h52m16s, Delta=+17d16' (1950.0) was surveyed with the Very Large Array at 1.452 GHz. The rms map noise is 0.030 + 0.001 mJy, and the resulting source list is complete to a map peak flux density S_p = 0.2 mJy within 25 arcmin of the field center. Source counts between 0.2 and 5 mJy were determined. Our best-fit model for the counts suggests that the faintest sources have absolute radio luminosities L < 10^24 W/Hz and do not evolve significantly. Sources stronger than 0.2 mJy appear to account for most of the radio-source background. The rms sky-temperature fluctuation in the central 10'x10' of the map is less than 0.029 K (>99% confidence) on an angular scale ~19 arcsec. This limit constrains theories which attribute the cosmic microwave background to thermalized radiation from massive pregalactic stars or bursts of star formation in young galaxies.
List of radio sources Name Source name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s e_RAs Mean error on RAs s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec e_DEs Mean error on DEs arcsec S1452 Integrated Flux Density mJy e_S1452 Mean error on S1452 mJy MajAxis Half-intensity major axis arcsec MinAxis Half-intensity minor axis arcsec PA MajAxis position angle deg f Integrated attenuation factor --- fp Peak attenuation factor --- mapSp Map Peak flux density mJy Heinz Andernach IUE Vilspa Francois Ochsenbein CDS 1997 Feb 13 UNKNOWN UNKNOWN scanned by H.Andernach in September 1995 (catalog numbered R222 in his archive) J_AJ_87_1429.xml Stars of spectral type A and B in the southern galactic halo. I. UBV photometry J/AJ/87/1515 J/AJ/87/1515 UBV photometry of AB stars in halo Stars of spectral type A and B in the southern galactic halo. I. UBV photometry J R Pier Astron. J. 87 1515 1982 1982AJ.....87.1515P J/ApJS/53/791 : Spectroscopy of AB stars in southern halo (Pier, 1983) Chavira E., 1958, Bol. Obs. Tonantzintla y Tacubaya 2, No. 17, 15 (1958BOTT....2q..15C) Haro G. & Luyten W.J., 1962, Bol. Obs. Tonantzintla y Tacubaya 3, No. 22, 37 (1962BOTT....3...37H, cat. <III/74>) Philip A.G.D. & Sanduleak N., 1968, Bol. Obs. Tonantzintla y Tacubaya 4. No. 30, 253 (1968BOTT....4..253P) Preston G.W. & Shectman S.A. 1979, Annual report of the Director, Hale Observatories (Carnegie Institution of Washington, Washinton, DC) Slettebak A. & Brundage R.K., 1971, Astron. J., 76, 338 (1971AJ.....76..338S) Photometry, UBV Stars, halo The results of photoelectric UBV photometry of 234 AB stars in the southern galactic halo are presented. The stars were chosen from the Curtis Schmidt objective-prism survey of Preston and Shectman and comprise a sample of halo objects selected without kinematic bias. The majority of the stars lie in the region of the (U-B, B-V) plane occupied by field and globular cluster blue horizontal-branch stars.
UBV photometry CS Curtis Schmidt plate number and the star number assigned by Preston designation as he scanned the plates --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin GLON Galactic longitude deg GLAT Galactic latitude deg Class Spectral and apparent brightness classifications assigned by Preston number=1 b = bright, f = faint, m = medium, v= very --- Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag o_Vmag Number of UBV observations --- Names Other designations number=2 PHL numbers are from Haro and Luyten (1962BOTT....3...37H) PS from table2 of Philip and Sanduleak (1968BOTT....4..253P) SB numbers from Slettebak and Brundage (1971AJ.....76..338S) TS numbers from the southern Tonantzintla list of Chavira (1958) --- James Marcout, Patricia Bauer CDS 1995 Feb 02 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_87_1515.xml Complete samples of active extragalactic objects. I. A 1411-MHz VLA survey centered on alpha= 12h04min, delta= +11deg30min J/AJ/87/739 J/AJ/87/739 Active extragalactic objects Complete samples of active extragalactic objects. I. A 1411-MHz VLA survey centered on alpha= 12h04min, delta= +11deg30min J J Condon M A Condon C Hazard Astron. J. 87 739 1982 1982AJ.....87..739C Radio sources As one part of a program to detect complete samples of active extragalactic objects, the 3.36x10^-3^sr field centered on alpha=12h04mim, delta=+11deg30' (1950.0) was mapped with the Very Large Array at 1411MHz. Sixty-seven maps cover this field so that no point is more than 15arcmin from the nearest map center. The median map noise is 0.6mJy, and the 6sigma completeness limit is less than 6mJy over half of the survey field. The synthesized point-source response is an elliptical Gaussian 22x18arcsec between half-intensity points. The rms source-position uncertainties are ~1arcsec in each coordinate so that reliable optical identifications can be made on the basis of radio-optical position coincidence alone. The sky density of sources with flux densities 5<=S<150mJy and the angular-size distribution of sources between 30 and 150mJy were determined.
Map parameters Map Map designation --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin MajAxis Gaussian equivalent half-intensity major axis arcsec --- --- MinAxis Gaussian equivalent half-intensity minor axis arcsec PA Major-axis position angle deg rms rms map noise mJy FPeakL Map peak flux density limit mJy Source list Name Source name --- m_Name Multiplicity index on Name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s e_RAs rms uncertainty on right ascension s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec e_DEs rms uncertainty on declination arcsec F1.4GHz Integrated flux density mJy e_F1.4GHz rms uncertainty on F1411MHz mJy MajAxis Gaussian equivalent half-intensity major axis arcsec --- --- MinAxis Gaussian equivalent half-intensity minor axis arcsec PA Major-axis position angle deg f Integrated attenuation factor --- fp Peak attenuation factor --- FMap Map peak flux density mJy Map Map designation --- James Marcout, Patricia Bauer CDS 1997 Jan 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_87_739.xml A deep survey of galaxies J/AJ/88/1285 J/AJ/88/1285 A deep survey of galaxies A deep survey of galaxies R P Kirshner A Oemler P L Schechter S A Shectman Astron. J. 88 1285 1983 1983AJ.....88.1285K J/AJ/83/1549 : A study of field galaxies. I. (Kirshner+ 1978) J/AJ/95/1629 : [O III] emission in 2 field-galaxy surveys (Moody+ 1988) Galaxies, photometry Redshifts We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.
The galaxy sample. Field Field designation --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Fmag F magnitude mag J-F J-F colour index mag cz Velocity km/s Com Comments number=1 KOS sample, Kirshner et al., 1978 Cat. <J/AJ/83/1549> and Kirshner et al., 1979AJ.....84..951K --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_88_1285.xml Radio and optical observations of a complete sample of E and SO galaxies. III. A radio continuum survey at 2.7 and 5.0 GHz. J/AJ/89/53 J/AJ/89/53 E and SO galaxies survey at 2.7 and 5.0 GHz Radio and optical observations of a complete sample of E and SO galaxies. III. A radio continuum survey at 2.7 and 5.0 GHz. E M Sadler Astron. J. 89 53 1984 1984AJ.....89...53S Galaxies, optical Galaxies, radio Radio continuum Surveys This paper presents results from a continuum radio survey of a complete sample of 248 southern E and S0 galaxies. All the galaxies were observed at 2.7GHz (11cm) with the Parkes radio telescope, and those detected were reobserved at 5.0 GHz (6 cm). Thirty-seven galaxies were detected above a level of 25-30mJy, and a consideration of the background source density at 2.7GHz indicates that no more than two or three of these detections are due to background sources.
Galaxies detected in the radio survey. Name Galaxy name --- RAh Optical Right Ascension B1950 (hours) h RAm Optical Right Ascension B1950 (minutes) min RAs Optical Right Ascension B1950 (seconds) s DE- Optical Declination B1950 (sign) --- DEd Optical Declination B1950 (degrees) deg DEm Optical Declination B1950 (minutes) arcmin DEs Optical Declination B1950 (seconds) arcsec RAr.h Radio Right Ascension B1950 (hours) h RAr.m Radio Right Ascension B1950 (minutes) min RAr.s Radio Right Ascension B1950 (seconds) s DEr.- Radio Declination B1950 (sign) --- DEr.d Radio Declination B1950 (degrees) deg DEr.m Radio Declination B1950 (minutes) arcmin DEr.s Radio Declination B1950 (seconds) arcsec l_S11cm Limit flag on S11cm --- S11cm Integrated flux density at 11cm (2.7GHz) mJy u_S11cm Uncertainty flag (:) on S11cm --- e_S11cm rms uncertainty on S6cm mJy l_S6cm Limit flag on S6cm --- S6cm Integrated flux density at 6cm (5GHz) mJy u_S6cm Uncertainty flag on S6cm --- e_S6cm rms uncertainty on S6cm mJy Notes Individual notes --- Radio properties of galaxies in the sample Name Galaxy name --- l_S2.7GHz Limit flag on S2.7GHz number=1 Upper limit for undetected galaxies --- S2.7GHz Flux density at 2.7GHz (11cm) mJy l_S5GHz Limit flag on S5GHz number=1 Upper limit for undetected galaxies --- S5GHz Flux density at S5GHz (6cm) mJy l_logP2.7GHz Limit flag on logP2.7GHz --- logP2.7GHz Radio power at 2.7GHz [W/Hz] SI Spectral index of the detected galaxies --- e_SI rms uncertainty on SI --- James Marcout, Patricia Bauer CDS 1998 Oct 23 UNKNOWN UNKNOWN Prepared via OCR at CDS, and proof-read by Heinz Andernach (heinz@astro.ugto.mx). J_AJ_89_53.xml Complete samples of active extragalactic objects. III. A 1411 MHz VLA survey. J/AJ/90/1437 J/AJ/90/1437 Active Extragalactic Objects III Complete samples of active extragalactic objects. III. A 1411 MHz VLA survey. P H Coleman J J Condon C Hazard Astron. J. 90 1437 1985 1985AJ.....90.1437C J/AJ/87/739 : Active Extragalactic Objects I. (Condon+ 1982) J/AJ/87/1429 : Active Extragalactic Objects II (Condon+ 1982) Radio sources Three selected fields were observed with the Very Large Array (VLA) at 1411MHz as part of an ongoing project to compile complete samples of active extragalactic objects. The radio-source list for the field "A" centered on alpha=08h54m, delta=+17d30' is presented. 67 maps cover the area 3x3deg so that every point lies within at least one primary half-power beamwidth. The median map noise is 0.5mJy and the 6{sigma} completeness level is less than 6mJy over half the field. The synthesized point-source response is an elliptical Gaussian approximately 20x17" between half-intensity points. The areal density of sources with flux densities in the range 5<S<150mJy was determined. Optical identifications based on position coincidences with 90 objects brighter than B=~21.5 in the A and B survey fields are reported.
List of radio sources Name Source name --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s e_RAs Mean error on RAs s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec e_DEs Mean error on DEs arcsec S1411MHz Integrated Flux Density mJy e_S1411MHz Mean error on S1411MHz mJy MajAxis Half-intensity major axis arcsec MinAxis Half-intensity minor axis arcsec PA MajAxis position angle deg f Integrated attenuation factor --- fp Peak attenuation factor --- mapSp Map Peak flux density mJy Map Map designation (parameters in table1 of paper) --- Optical identifications Name Source name, as in tabl2 --- IDdir Identification by direct observation the symbols are G = Galaxy ; S = star-like object ; QSO = quasar ? = object of unknown nature --- IDop Identification by objective prism --- Bmag Blue magnitude determined by the APM mag u_Bmag Uncertainty flag (:) on Bmag --- dRA Offset in Right Ascension s dDE Offset in Declination arcsec m Normalized position difference difference between optical and radio positions divided by the errors in each; see Mitchell et al. (1981PASP...93..647M) for details on m definitions and statistics. --- Francois Ochsenbein CDS 1997 Feb 13 We thank Heinz Andernach <heinz@cuevano.ugto.mx> who scanned and proofread the tables (numbered R196 in his archive) J_AJ_90_1437.xml A complete VLA survey in the outer galaxy. J/AJ/92/787 J/AJ/92/787 Outer galaxy VLA survey A complete VLA survey in the outer galaxy. M Fich Astron. J. 92 787 1986 1986AJ.....92..787F VII/20 : Catalogue of HII Regions (Sharpless 1959) VII/50 : CO Radial Velocities Toward Galactic H II Regions (Blitz+ 1982) H II regions Radio lines Radio sources The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).
Catalog of radio sources Name Source designation number=1 KR refers to Kallas & Reich (1980A&AS...42..227K) S refers to Sharpless (1959, Cat. <VII/20>) W refers to Westerhout (1958BAN....14..215W) SNR refers to an unnamed supernova remnant --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec S1.42GHzp Peak 1.42GHz flux Jy S1.42GHz Total 1.42GHz flux Jy n_S1.42GHz Note on S1.42GHz number=2 n: no detection, c: confused, v: very strong,confused, w: very weak o: outside of 2cm field, b: observed wrong position e: flux estimated from maps, else from Kallas & Reich (1980A&AS...42..227K) catalog --- S4.89GHzp Peak 4.89GHz flux mJy S4.89GHz Total 4.89GHz flux mJy n_S4.89GHz Note on S4.89GHz (2) number=4 *: a correction has been applied. The 4.89GHz fluxes have been corrected for primary-beam attenuation (PBAF) and bandwidth smearing (BWSAF) as follow: KR22 : PBAF = 1.83, BWSAF = 2.3 KR71 B: PBAF = 1.21, BWSAF = 1.33 KR71 C: PBAF = 1.18, BWSAF = 1.28 KR71 D: PBAF = 1.14, BWSAF = 1.22 S167 : confused with Cas A SNR KR93 B: PBAF = 2.13, BWSAF = 2.83 KR100 : PBAF = 1.25, BWSAF = 1.39 KR128 : PBAF = 1.14, BWSAF = 1.22 KR147A: PBAF = 1.25, BWSAF = 1.40 KR147B: PBAF = 2.04, BWSAF = 2.70 KR155 : PBAF = 1.12, BWSAF = 1.19, 2 jets and halo, ext 90"x30" KR178 : PBAF = 1.15, BWSAF = 1.24 KR186 : core + 2 jets, 35"x10" KR193 : PBAF = 1.12, BWSAF = 1.17 KR204 : can not separate two components at 2cm KR212 : PBAF = 1.13, BWSAF = 1.18, over-resolved, see text KR221 : PBAF = 1.28, BWSAF = 1.44 KR228 : PBAF = 1.57, BWSAF = 1.91, flux missing KR235A: PBAF = 1.15, BWSAF = 1.22 KR235B: PBAF = 1.25, BWSAF = 1.39 --- S14.96GHzp Peak 14.96GHz flux mJy S14.96GHz Total 14.96GHz flux mJy n_S14.96GHz Note on S14.96GHz number=2 n: no detection, c: confused, v: very strong,confused, w: very weak o: outside of 2cm field, b: observed wrong position e: flux estimated from maps, else from Kallas & Reich (1980A&AS...42..227K) catalog --- SI Spectral index between 4.89 and 14.96 GHz. --- Com Comments number=3 Comments, including other names for the object (BFS refers to the catalog of Blitz et al., 1982, Cat. <VII/50>) and details about the structure seen, size scales, and type of object (e.g., HII means H II region). If no size is given, the object was not resolved. --- Indiviudal notes (for KR objects only) Name Object name --- Note Text of the note --- James Marcout, Patricia Bauer CDS 1998 Dec 19 UNKNOWN UNKNOWN * December 1998: Prepared via OCR at CDS. Proof-read and corrections by Heinz Andernach (heinz@astro.ugto.mx) Misprint: HB 3: Declination changed from +62 77 39.0 to +62 17 39.0 J_AJ_92_787.xml The [O III] emission in two magnitude-limited field-galaxy surveys J/AJ/95/1629 J/AJ/95/1629 [O III] emission in 2 field-galaxy surveys The [O III] emission in two magnitude-limited field-galaxy surveys J W Moody R P Kirshner Astron. J. 95 1629 1988 1988AJ.....95.1629M J/AJ/83/1549 : A study of field galaxies. I. (KOS) (Kirshner+ 1978) J/AJ/88/1285 : A deep survey galaxies. (KOSS) (Kirshner+ 1983) Equivalent widths Galaxies, spectra We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. <J/AJ/83/1549>, KOS) and Kirshner et al. (1983, Cat. <J/AJ/88/1285>, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. <J/J/83/1549>) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.
KOS (1978AJ.....83.1549K) survey data Field Field designation --- Obj Object number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec MType Morphological type --- Jmag Visual J magnitude mag J-F J-F colour index mag JMag Absolute J magnitude mag cz Velocity km/s EW3727 [O II] {lambda}3727{AA} equivalent width number=2 A blank indicates that the coverage did not include that line H{alpha} is often H{alpha}, [N II] blend 0.1nm n_EW3727 Note on EW3727 number=3 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- Note1 Note on emission number=1 a: Emission contaminated by cosmic ray b: Emission from a southern HII region on photographic plate was not found by follow-up reticon scan. --- l_EWHbeta Limit flag on EWHbeta --- EWHbeta H{beta} equivalent width number=2 A blank indicates that the coverage did not include that line H{alpha} is often H{alpha}, [N II] blend 0.1nm n_EWHbeta Note on EWHbeta number=3 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- Note2 Note on emission number=1 a: Emission contaminated by cosmic ray b: Emission from a southern HII region on photographic plate was not found by follow-up reticon scan. --- l_EW4959 Limit flag on EW4959 --- EW4959 [O III] {lambda}4959{AA} equivalent width number=2 A blank indicates that the coverage did not include that line H{alpha} is often H{alpha}, [N II] blend 0.1nm n_EW4959 Note on EW4959 number=3 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- Note3 Note on emission number=1 a: Emission contaminated by cosmic ray b: Emission from a southern HII region on photographic plate was not found by follow-up reticon scan. --- l_EW5007 Limit flag on EW5007 --- EW5007 [O III] {lambda}5007{AA} equivalent width number=2 A blank indicates that the coverage did not include that line H{alpha} is often H{alpha}, [N II] blend 0.1nm n_EW5007 Note on EW5007 number=3 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- Note4 Note on emission number=1 a: Emission contaminated by cosmic ray b: Emission from a southern HII region on photographic plate was not found by follow-up reticon scan. --- EWHalpha H{alpha} equivalent width number=2 A blank indicates that the coverage did not include that line H{alpha} is often H{alpha}, [N II] blend 0.1nm n_EWHalpha Note on EWHalpha number=3 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- Note5 Note on emission number=1 a: Emission contaminated by cosmic ray b: Emission from a southern HII region on photographic plate was not found by follow-up reticon scan. --- Ref References number=4 References 1: McGraw-Hill 1.3m, Mark II, Jan 84, range=3700-7500, mag tape 2: McGraw-Hill 1.3m, Mark II, Apr 84, range=3700-7500, mag tape 3: KPNO 0.9m, image tube spectrograph, Spring 77, range=3500-7000, redshift emission-line lists, photographic plates 4: KPNO 2.1m, IDS, May 77, range=3700-7000, redshift emission line lists 5: McGraw-Hill 1.3m, Mark I, May 78, range=3700-7500, magnetic tape 6: McGraw-Hill 1.3m, Mark II, May 78, range=3700-7500, redshift emission line lists 7: CTI0 Yale 1.0m, image tube spectrograph, range=3500-7000, photographic plates 8: Palomar 5m, SIT spectrograph, Oct 79, range=3850-5450, plot 9: Palomar 5m, double spectrograph, Sep 79, range=3700-5400, plot 10: McGraw-Hill 1.3m, Mark II, March 85, range=3750-5500, mag tape 11: McGraw-Hill 1.3m, Mark II, April 85, range=3700-7000, mag tape 12: McGraw-Hill 1.3m, Mark III-RCA CCD, Sep 85, range=4350-5570, mag tape 13: McGraw-Hill 1.3m, Mark III-RCA CCD, Sep 85, range=3700-7000, mag tape --- Com Comment ---- KOSS (1983AJ.....88.1285K) survey data Field Field designation --- Obj Object number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Jmag Visual J magnitude mag u_Jmag ')' when estimated magnitude --- J-F J-F colour index mag u_J-F ')' when estimated color index --- JMag Absolute J magnitude mag u_JMag ')' when estimated magnitude --- cz Velocity km/s EW3727 [O II] {lambda}3727{AA} equivalent width 0.1nm n_EW3727 Note on EW3727 number=1 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- EWHbeta H{beta} equivalent width 0.1nm n_EWHbeta Note on EWHbeta number=1 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- l_EW4959 Limit flag on EW4959 --- EW4959 [O III] {lambda}4959{AA} equivalent width 0.1nm n_EW4959 Note on EW4959 number=1 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- l_EW5007 Limit flag on EW5007 --- EW5007 [O III] {lambda}5007{AA} equivalent width 0.1nm n_EW5007 Note on EW5007 number=1 N: the line was not detected at the noise level of the spectrum D: the line was detected but no equivalent width was measured --- Ref References number=2 References: 1: McGraw-Hill 1.3m, Mark II, Apr 84, range=3700-7500, mag tape 2: McGraw-Hill 1.3m, Mark II, Jan 84, range=3700-7500, mag tape 3: KPNO 2.1m, IDS, Jun 79, range=3700-5450, mag tape 4: Las Campanos 2.3m, IDS, Dec 79, range=3700-6400, mag tape 5: Palomar 5m, digital spectrograph, June 80, reticon, range=3850-4850, mag tape 6: Palomar 5m, SIT spectrograph, Oct 79, range=3850-5450, plot 7: Palomar 5m, SIT spectrograph, May 79, range=3850-5450, AB mag plot 8: Unknown, range=3580-4800, plot 9: Palomar 5m, double spectrograph, Sep. 79, range=3700-5400, plot 10: Los Campanos 2.3m, reticon spectrograph, Sep. 79, range=3000-6600, mag tape 11: Palomar 5m, digital spectrograph, Oct 80, range=3750-4950, plot 12: McGraw-Hill 1.3m, Mark I, March 77, range=4800-5800, mag tape 13: McGraw-Hill 1.3m, Mark III-RCA CCD, Sep 85, range=4350-5570, mag tape --- Com Comment ---- Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 18 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_95_1629.xml A color-magnitude diagram for the halo globular cluster M 55 J/AJ/96/1632 J/AJ/96/1632 CCD BV photometry in M55 A color-magnitude diagram for the halo globular cluster M 55 D Schade D A VandenBerg F D A Hartwick Astron. J. 96 1632 1988 1988AJ.....96.1632S Clusters, globular Photometry, CCD We present new CCD photometry for the globular cluster M55 that extends well below the main-sequence turnoff. Combining these new data with previously published photographic photometry of cluster giants and horizontal-branch stars yields a high-quality composite color-magnitude diagram (CMD). A comparison of the latter with recent CMDs for M68 and NGC 6752-two clusters whose metallicities bracket that of M55-suggests (1) that the reddening to M55 may be as high as E(B-V)=0.14mag, and (2) that all three systems have similar ages. In particular, if the apparent distance modulus to M55 is (m-M)_V_=14.10mag, then isochrones for Y=0.24 and high [O/Fe] would suggest an age of ~14Gyr. Very encouraging agreement of the observations with theoretical predictions is found.
M 55 NGC 6809 19 39 59.3 -30 57 44
CCD photometry in M 55 Star Star number --- Xpos X position number=1 1 pix = 0.44"; X positive from West to East, Y from South to North. pix Ypos Y position number=1 1 pix = 0.44"; X positive from West to East, Y from South to North. pix Vmag V magnitude mag B-V B-V colour index mag Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 18 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_96_1632.xml A VLA snapshot continuum survey of the first quadrant of the galactic plane at 1.5 GHz. J/AJ/96/1655 J/AJ/96/1655 Galactic plane VLA survey A VLA snapshot continuum survey of the first quadrant of the galactic plane at 1.5 GHz. R W Garwood R A Perley J M Dickey M A Murray Astron. J. 96 1655 1988 1988AJ.....96.1655G Galactic plane Radio sources Surveys We present results from a continuum VLA snapshot survey of the galactic plane in the longitude range 0{deg}<=l<=90{deg} at 1.5GHz. Observations were taken every 0.5{deg} in longitude at b=0{deg}. Most fields are complete to about 30mJy peak flux density. The positions, peak, and total flux density of 471 compact sources (<30") have been measured. A complete sample of 329 sources is defined. An excess of sources above that expected from extragalactic source counts is seen for l<40{deg} at all flux-density intervals. We find 86 compact sources that are within 2.4arcmin of a source in the recent radio recombination-line survey of Lockman (1989ApJS...71..469L) Source counts excluding these 86 sources agree with extragalactic source counts for all flux-density and longitude intervals. there may only be a small number of galactic objects present in this survey that remain unidentified as such.
Source list GLON Galactic longitude deg GLAT Galactic latitude deg Slim Completeness limit number=1 Completness limit (uncorrected for primary-beam attenuation and bandwidth smearing) corresponding to the field on which the source was found. mJy RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Sint Integral flux density mJy Speak Peak flux density (in mJy/beam) mJy Sint/Speak Ratio of integral to peak flux density --- F1 Center flag number=2 F1=1 if the source is within 15arcmin from the pointing center, otherwise F1=0 --- F2 Completeness flag number=3 F2=1 if the the uncorrected source peak flux density is greater than the completeness limit of the field, otherwise F2=0 --- Note Note about other surveys number=4 A: Survey position is less than 2.6' from the source in Altenhoff et al. (1979A&AS...35...23A) L: Survey position is less than 2.4' from a recombination-line source in Lockman (1989ApJS...71..469L) I: Interesting IR source found at survey position by Jones, Garwood and Dickey (1988ApJ...328..559J) H: 21cm absorption towards this source by Garwood and Dickey (1989ApJ...338..841G) --- Com Comments --- Francois Ochsenbein CDS 1997 May 05 Thanks are due to Heinz Andernach <hja@vilspa.esa.es> who forwarded his copy (catalog numbered R115 in his list) J_AJ_96_1655.xml The red supergiants in M31: spectra, colors, and luminosities J/AJ/96/1884 J/AJ/96/1884 BVRJHK photometry of M31 red supergiants The red supergiants in M31: spectra, colors, and luminosities R M Humphreys R L Pennington T J Jones F D Ghigo Astron. J. 96 1884 1988 1988AJ.....96.1884H II/144 : Brightest stars in the field of M31 (Berkhuijsen+ 1988) II/145 : Brightest stars in a foreground field of M31 (Berkhuijsen+, 1988) Photometry, infrared Stars, supergiant We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.
Red stars in M31: positions, magnitudes,and colors Star Star designation number=1 Star R-1 has been retried of table1. It has no coordinates because it is at the edge of plate (the only data is Assoc = 103) --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V color index mag e_B-V rms uncertainty on B-V mag V-R V-R color index mag e_V-R rms uncertainty on V-R mag Year Year minus 1900 yr n_Year a: average --- J-H J-H color index mag u_J-H Uncertainty flag on J-H --- e_J-H rms uncertainty on J-H mag H-K H-K color index mag u_H-K Uncertainty flag on H-K --- e_H-K rms uncertainty on H-K mag Kmag K magnitude mag u_Kmag Uncertainty flag on Kmag --- e_Kmag rms uncertainty on Kmag mag Assoc Association number number=2 Number of association from Van den Berg (1964ApJS....9...65V) --- Rem Remarks --- Cat. Catalogue number number=3 Number from Berkhuijsen et al. (1988, Cat. <II/144> and <II/145>) --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 17 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_96_1884.xml CCD photometry of the anomalous globular cluster Palomar 12 J/AJ/97/1360 J/AJ/97/1360 BV photometry of Palomar 12 CCD photometry of the anomalous globular cluster Palomar 12 P B Steton D A VandenBerg M Bolte J E Hesser G H Smith Astron. J. 97 1360 1989 1989AJ.....97.1360S Clusters, globular Photometry, CCD We present broadband B,V photometry for 1154 stars in the field of the Galactic globular cluster Palomar 12, based upon direct CCD images obtained with the Canada-France-Hawaii 3.6m and Cerro Tololo 4m telescopes. The overall zero points of our V magnitudes and B-V colors appear to be known to about +/-0.02mag and +/-0.01mag, and our magnitude- and color-scale errors are probably controlled to <0.01mag. Pal 12's main sequence shows an excess fringe of stars along its red edge which are probably binaries; the CM diagram also contains a small number of probable blue stragglers. The principal result of this paper is that the color-magnitude diagram of Pal 12 is anomalous, in the sense that we cannot fake all of its principal sequences lie near or between those of the well studied and presumably typical Galactic globular clusters 47 Tucanae and M5, even though it lies near or between them in overall heavy-element abundance. The simplest explanation is that Pal 12 is younger than the other two clusters by some 25-30%. Other explanations are also possible, although perhaps somewhat harder to believe. This result greatly strengthens the possibility that age differences are responsible, at least in part, for the anomalous properties of some of the outer-halo globular clusters. Spectroscopic indications are that Pal 12's chemical abundances should also strongly resemble those of the two Galactic globular clusters NGC 288 and NGC 362, which have also been claimed to show age differences in comparison with M5. However, attempts to derive ages for these clusters relative to M5 and Pal 12 are inconclusive, possibly due to some inconsistencies within the available data.
Palomar 12 C 2143-214 21 46.5 -21 14
Photometry for stars in Pal 12. ID Star number number=1 ID < 5000: stars measured by Harris et Canterna (1980ApJ...239..815H) ID > 5000: Object not measured by Harris et Canterna (1980) --- Xpos X position number=2 X increasing from South to North, Y increasing from West to East 1 pix = 0.20" pix Ypos Y position number=2 X increasing from South to North, Y increasing from West to East 1 pix = 0.20" pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag o_Vmag Number of observation in Vmag number=3 Total number of frames in each pass-band in which the star was measurable. --- o_Bmag Number of observation in Bmag number=3 Total number of frames in each pass-band in which the star was measurable. --- <Chi> Mean of the goodness of fit index --- <r0> Mean of the image radius index number=4 Positive when an object appears to be more extended than the model stellar profile for the frame Negative when the detection appears sharper than a star image pix Marie-Jose Wagner, Patricia Bauer CDS 1997 May 05 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_97_1360.xml A VLA survey of the 3 clusters of galaxies 0016+16, Abell 665, and Abell 2218. J/AJ/98/1148 J/AJ/98/1148 VLA survey of 0016+16, Abell 665, and Abell 2218 A VLA survey of the 3 clusters of galaxies 0016+16, Abell 665, and Abell 2218. A T Moffet M Birkinshaw Astron. J. 98 1148 1989 1989AJ.....98.1148M Clusters, galaxy Galaxies, radio We have used the VLA to survey the fields of the three clusters of galaxies; 0016+16, Abell 665 (0826+66) and Abell 2218 (1635+66) at 1440 MHz, 4860 MHz, and 14940 MHz (for the brighter sources). The survey was aimed at finding radio sources which might contaminate the Sunyaev-Zel'dovich effect. We have detected 86 sources in these three clusters and examined Palomar sky survey prints for possible optical identifications.
VLA Survey of 3 Clusters of Galaxies: 0016+16, A665, and A2218 Cluster Name of cluster number=1 These columns give the name of the cluster which contains the source and the number of the source within the field. The sources are numbered independently for each of the 3 clusters. --- Seq Sequential number of source number=1 These columns give the name of the cluster which contains the source and the number of the source within the field. The sources are numbered independently for each of the 3 clusters. --- RAh Right Ascension 1950 (hours) number=2 These columns give the B1950 position of the source The positions were combined from measurements at each frequency, taking account of possible systematic, frequency-dependent errors in the locations of the radio centroids. Where the source was clearly resolved, the center of the radio emission (either the location of a point source, or the midpoint of extended lobes) was used for the source position. h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s e_RAs Error on right ascension s DE- Declination 1950 (sign) number=2 These columns give the B1950 position of the source The positions were combined from measurements at each frequency, taking account of possible systematic, frequency-dependent errors in the locations of the radio centroids. Where the source was clearly resolved, the center of the radio emission (either the location of a point source, or the midpoint of extended lobes) was used for the source position. --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec e_DEs Error on declination arcsec l_S1440 Flux density flag at 1440 MHz number=3 flagged with a "<" when the corresponding flux densities are upper limits. --- S1440 Flux density at 1440 MHz number=4 These columns give the flux density at 1440 MHz, 4860 MHz, and 14940 MHz, in mJy. The flux density scale is that of Baars, et. al (1977A&A....61...99B). It is important to note that these fields were not systematically observed at 15 GHz; only the strongest sources were targeted at that frequency. mJy e_S1440 Error on 1440 MHz flux density mJy l_S4860 Flux density flag at 4860 MHz number=3 flagged with a "<" when the corresponding flux densities are upper limits. --- S4860 Flux density at 4860 MHz number=4 These columns give the flux density at 1440 MHz, 4860 MHz, and 14940 MHz, in mJy. The flux density scale is that of Baars, et. al (1977A&A....61...99B). It is important to note that these fields were not systematically observed at 15 GHz; only the strongest sources were targeted at that frequency. mJy e_S4860 Error on 4860 MHz flux density mJy l_S14940 Flux density flag at 14940 MHz number=3 flagged with a "<" when the corresponding flux densities are upper limits. --- S14940 Flux density at 14940 MHz number=4 These columns give the flux density at 1440 MHz, 4860 MHz, and 14940 MHz, in mJy. The flux density scale is that of Baars, et. al (1977A&A....61...99B). It is important to note that these fields were not systematically observed at 15 GHz; only the strongest sources were targeted at that frequency. mJy e_S14940 Error on 14940 MHz flux density mJy l_MajAxis Flag for major axis number=5 These columns are flagged with a "<" when the corresponding major and minor axes sizes are upper limits. --- MajAxis Angular size of major axis number=6 These columns give the angular size and position angle of the sources. The major and minor axes are listed independently, in arcsec, and the position angle is listed in degrees. arcsec l_MinAxis Flag for minor axis number=5 These columns are flagged with a "<" when the corresponding major and minor axes sizes are upper limits. --- MinAxis Angular size of minor axis number=6 These columns give the angular size and position angle of the sources. The major and minor axes are listed independently, in arcsec, and the position angle is listed in degrees. arcsec PA Position angle number=6 These columns give the angular size and position angle of the sources. The major and minor axes are listed independently, in arcsec, and the position angle is listed in degrees. deg Comments Radio and Optical comments number=7 This column gives radio and optical comments on the source, separated by a semi-colon where both are given. Where reference is made to a figure, the original paper listed that reference in the angular size column and this reference has been moved to the comments column for the electronic version of this catalogue. See the published paper for the figures. --- RAoh Optical counterpart Right Asc. (B1950) number=8 These columns give the B1950 position and error of the optical candidate of the source. h RAom Optical count. Right Ascension (B1950)(min) min RAos Optical count. Right Ascension (B1950)(sec) s e_RAos Error on optical RA number=8 These columns give the B1950 position and error of the optical candidate of the source. s DEo- Optical counterpart Declination sign (B1950) number=8 These columns give the B1950 position and error of the optical candidate of the source. --- DEod Optical count. Declination (B1950)(deg) deg DEom Optical count. Declination (B1950)(arcmin) arcmin DEos Declination (B1950) (arcsec) arcsec e_DEos Error on optical declination number=8 These columns give the B1950 position and error of the optical candidate of the source. arcsec Patricio Ortiz CDS 1999 Mar 30 UNKNOWN UNKNOWN "The catalogue was originally archived as A010 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_AJ_98_1148.xml The stellar content of NGC 346: a plethora of O stars in the SMC J/AJ/98/1305 J/AJ/98/1305 Stellar content of NGC 346 The stellar content of NGC 346: a plethora of O stars in the SMC P Massey J W Parker C D Garmany Astron. J. 98 1305 1989 1989AJ.....98.1305M H II regions Magellanic Clouds Nebulae Spectrophotometry Stars, O Stars, Wolf-Rayet Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.
Photometry of NGC 346 Id Star number --- Xpos X position pix Ypos Y position pix Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag number=1 A colon indicates measurement whose error is twice as big as that given in table3, two colons denote those stars whose photometry has errors which are >=3{sigma}. In addition, colons are used to denote stars whose photometry is outside the range well fit by colour transformations. --- U-B U-B colour index mag u_U-B Uncertainty flag on U-B number=1 A colon indicates measurement whose error is twice as big as that given in table3, two colons denote those stars whose photometry has errors which are >=3{sigma}. In addition, colons are used to denote stars whose photometry is outside the range well fit by colour transformations. --- B-V B-V colour index mag u_B-V Uncertainty flag on B-V number=1 A colon indicates measurement whose error is twice as big as that given in table3, two colons denote those stars whose photometry has errors which are >=3{sigma}. In addition, colons are used to denote stars whose photometry is outside the range well fit by colour transformations. --- Comparison with Niemela et al. (1986) Id Star number --- m_Id Other star numbers when multiple star --- NameN Niemela star number --- Vmag V magnitude from this work mag u_Vmag Uncertainty flag on Vmag --- VmagN V magnitude from Niemela mag Rem Remarks number=1 *: also identified as multiple by Niemela et al. --- Other bright stars in NGC 346 Id Star number --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Xpos X position pix Ypos Y position pix Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag --- U-B U-B colour index mag u_U-B Uncertainty flag on U-B --- B-V B-V colour index mag u_B-V Uncertainty flag on B-V --- Com Comments number=1 References: PMMRR = Prevot et al. (1983) Sanduleak = Sanduleak (1989) --- Marie-Jose Wagner, Patricia Bauer CDS 1995 Mar 02 UNKNOWN UNKNOWN Keypunched at CDS J_AJ_98_1305.xml Subdwarf studies. I. UBVRI photometry of NLTT stars. J/AJ/98/1693 J/AJ/98/1693 UBVRI photometry of NLTT stars Subdwarf studies. I. UBVRI photometry of NLTT stars. S G Ryan Astron. J. 98 1693 1989 1989AJ.....98.1693R I/98 : Luyten's NLTT Catalog Photometry, UBVRI Stars, subdwarf UBVRI photometry is presented for a sample of 1656 southern stars, including 1211, that were previously not measured, drawn from the NLTT (Luyten, 1979; catalogue <I/98>) proper-motion catalog; the catalog is shown to be a rich source of subdwarfs. The normalized UV excess, d(U-B)0.6, photometric parallax, and interstellar reddening are calculated for each star when possible. Residuals between the photometry and the magnitudes published in the NLTT catalog indicate that the latter have a large scatter (~0.6mag) and therefore the values tabulated in the NLTT catalog must be regarded as approximate only. The erratum (Astron. J. 99, 1336) which deals with position angles of proper motions (pmPA) has been taken into account.
Observed photometry and derived parameters Name Name of the star, as in NLTT number=1 Identifiers without prefixes are DM (Bonner and Cordoba Durchmusterungen, written with a colon), or Luyten numbers from the Bruce Proper Motion Survey (L numbers) or the Luyten-Palomar Survey (LP numbers), the former in zones -45 to -89 deg and the latter in zones +89 to -44 deg. Other miscellaneous identifiers (Oxf = Oxford AC, Grw = Greenwich AC; U = Upgren; R = Ross, etc...). An asterisk (*) in the identification field indicates that a note exists in the "remarks" file of the NLTT <I/98> catalog. --- RAh Right Ascension 1950 (hours), Epoch=1950 h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec pm Annual total proper motion number=5 The total proper motion is reported. The RA/DE proper motions can be computed with the formulae pmRA = pm.sin(pmPA) pmDE = pm.cos(pmPA) arcsec/yr pmPA Position angle of proper motion number=5 The total proper motion is reported. The RA/DE proper motions can be computed with the formulae pmRA = pm.sin(pmPA) pmDE = pm.cos(pmPA) deg Vmag Magnitude of UBV system mag B-V colour index mag U-B colour index mag d(U-B)0.6 Normalized ultraviolet excess number=2 Colour excess as defined in Sandage (1969ApJ...158.1115S) mag V-R colour index mag R-Ic colour index (I in Cousins) mag Nobs Number of observations --- ACflag Ambiguity / Contamination note number=3 (only when Nobs is blank) 'A' denotes 36 stars that could not be unambiguously identified from the coordinates or photometric data 'C' denotes 22 stars with visible close companions that would have contaminated photometry. --- Dist Photometric distance pc u_Dist Uncertainty flag (:) on Dist --- E(B-V) Derived colour excess mag u_E(B-V) Uncertainty flag (:) on E(B-V) --- d(U-B)' De-reddened normalized ultraviolet excess mag inTable4 '*' when the star is also in table4 --- Note Note/Trigonometric parallax note number=4 this note has the following meaning: 'N' when a note exists at the end of the published table 'T' when a trigonometric parallax is listed in the published Table 7 --- OtherNames Alternate designations of the star --- Photometry from literature and derived parameters Name Name of the star, as in NLTT number=1 See note (1) for table3 --- RAh Right Ascension 1950 (hours), Epoch=1950 h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec pm Annual total proper motion number=5 The total proper motion is reported. The RA/DE proper motions can be computed with the formulae pmRA = pm.sin(pmPA) pmDE = pm.cos(pmPA) arcsec/yr pmPA Position angle of proper motion number=5 The total proper motion is reported. The RA/DE proper motions can be computed with the formulae pmRA = pm.sin(pmPA) pmDE = pm.cos(pmPA) deg Vmag Magnitude of UBV system mag B-V colour index mag U-B colour index mag d(U-B)0.6 Normalized ultraviolet excess number=2 Colour excess as defined in Sandage (1969ApJ...158.1115S) mag R-Ic colour index (I transformed from Kron to Cousins) mag Ref Reference of the Photometry number=3 References are: CL = Carney & Latham (1987AJ.....93..116C) E1 = Eggen O.J. (1979ApJS...39...89E) E2 = Eggen O.J. (1980ApJS...43..457E) E3 = Eggen O.J. (1987AJ.....93..379E) SF = Sandage & Fouts (1987AJ.....93...74S) SK = Sandage & Kowal (1986AJ.....91.1140S) S2 = Sandage (1969ApJ...158.1115S) --- Dist Photometric distance pc u_Dist Uncertainty flag (:) on Dist --- E(B-V) Derived colour excess mag u_E(B-V) Uncertainty flag (:) on E(B-V) --- d(U-B)' De-reddened normalized ultraviolet excess mag Note Note number=4 this note has the following meaning: '*' when the star is also in table3 'N' when a note exists at the end of the published table 'T' when a trigonometric parallax is listed in the published Table 7 'S?' indicates as suspected binary 'SB' indicates a probable binary 'DB' indicates a double-lined system --- OtherNames Alternate designations of the star --- Notes on individual stars Name Name of the star, as in NLTT --- RAh Right Ascension 1950 (hours), Epoch=1950 h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Text Text of note; the prefix G: indices a note from LPMS (Luyten's Proper Motion Survey) --- Francois Ochsenbein CDS 1995 Dec 01 Thanks are due to Heinz J. Andernach for contacting the author, and reformatting the tables. The notes have been typed by J. Marcout [CDS] Sean Ryan, Anglo-Australian Observatory <SGR@aaoepp2.aao.gov.au> J_AJ_98_1693.xml CCD photometry of the RR Lyrae variables in the LMC cluster NGC 2257 and the adjacent field J/AJ/98/2086 J/AJ/98/2086 CCD photometry of NGC 2257 RR Lyrae CCD photometry of the RR Lyrae variables in the LMC cluster NGC 2257 and the adjacent field A R Walker Astron. J. 98 2086 1989 1989AJ.....98.2086W Photometry, CCD Stars, variable Extensive B and V band CCD photometry for 33 cluster and nine field RR Lyrae variables near the old LMC cluster NGC 2257 provide accurate mean magnitudes for the stars, and hence distances for the cluster and field populations. The mean magnitudes for the two groups differ by 0.17mag. This is interpreted as a distance effect rather than a difference in metal abundance or evolutionary state. The field stars thus average 3.7kpc more distant from us than cluster stars, and 4.1kpc more distant than the plane of the LMC as defined by the de Vaucouleurs and Freeman incline plane model. In addition the field stars occupy less than 9kpc in depth; however, the data are not inconsistent with the LMC field RR Lyrae, taken as a whole, forming a spherical rather than a planar system. From the period-amplitude diagram, both the cluster and field variables have metal abundance of [Fe/H]=-1.8+/-0.1. There is little evidence for any gross spread in metal abundance among the field variables, although periods for two short-period and, presumably, metal-rich RRab stars are confirmed. The new light curves extend previous work on period changes for the cluster variables and have allowed revised periods and rates of period change to be calculated. Two possible double-mode (RRd) field variables were found to have incorrect periods and are actually RRabb stars. Photometry for 462 stars, reaching to V~21 and sampling the cluster to its very center, have been used to prepare a color-magnitude of the evolved stars in NGC 2257. This shows a richly populated blue horizontal branch, the width of which measurements of the dispersion of absolute magnitudes of RR Lyrae in galactic globular clusters by Sandage. The asymptotic giant branch is early separated from the red giant branch allowing accurate numbers of stars in the various stages of evolution to be counted. These counts are compared with those for galactic globular clusters, with the result that NGC 2257 appears to be indistinguishable from its local counterparts such as M3.
NGC 2257 06 30.4 -64 19
Photometry for the NGC 2257 non-variables Seq Star sequential number --- Xoff X offset from star 78 (Alcaino I) (+ is West) number=1 Alcaino I in Alcaino & Alvarado, 1988AJ.....95.1724A. arcsec Yoff Y offset from star 78 (Alcaino I) (+ is North) number=1 Alcaino I in Alcaino & Alvarado, 1988AJ.....95.1724A. arcsec Vmag V magnitude mag B-V B-V colour index mag Derived properties of the NGC 2257 variables Derived properties of the field variables Star Star number --- Per Period number=1 The period given here is that adopted by NHH (Nemec et al., 1985ApJS...57..329), and corresponds to the epoch given by these authors (Tables V, VI of Nemec et al., 1985ApJS...57..329). The phase at maximum light in February 1988 (column Phase) corresponds to this ephemeris. See text for revised periods and period change rates for many of these stars. d Type Variable type --- <Vmag> Intensity mean V magnitude mag u_<Vmag> Uncertainty flag on <Vmag> --- <Bmag> Intensity mean B magnitude mag u_<Bmag> Uncertainty flag on <Bmag> --- <Bmag>-<Vmag> <Bmag> minus <Vmag> mag u_<Bmag>-<Vmag> Uncertainty flag on <Bmag>-<Vmag> --- <B-V> B-V magnitude mean mag u_<B-V> Uncertainty flag on <B-V> --- AV V amplitude mag u_AV Uncertainty flag on AV --- AB B amplitude mag u_AB Uncertainty flag on AB --- Rise Rise time to maximum (in phase units) --- u_Rise Uncertainty flag on Rise --- Phase Phase at the maximum light --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 29 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_98_2086.xml Structures, spectral indexes, and optical identifications of radio sources selected from the B3 catalogue. J/AJ/98/419 J/AJ/98/419 Observed quantities from B3 sources Structures, spectral indexes, and optical identifications of radio sources selected from the B3 catalogue. M Vigotti G Grueff R Perley B G Clark A H Bridle Astron. J. 98 419 1989 1989AJ.....98..419V VIII/37 : The Third Bologna Survey (B3) Kron, 1986, Private communication Radio sources This catalog contains results of a large program of optical identifications of radio sources from the Third Bologna (B3) Catalog (Ficarra et al., 1985A&AS...59..255F, Cat.<VIII/37>). A homogeneous sample of 1103 radio sources, selected from the B3 catalog at 408 MHz and covering a flux density range from 2.0 to 0.1 Jy, has been mapped at 1465 MHz using the VLA at 15" resolution. Both positional and structural information have been derived and are presented here. Optical identifications have been attempted for all of the sources within the range of right ascension studied, using the Palomar Sky Survey prints, resulting in 354 proposed identifications. The RA range was restricted to exclude sky areas at low galactic latitude, because obscuration makes these unsuitable for optical identifications, and confusion makes them unsuitable for VLA snapshot-mode observations. Thus the samples were selected only from the RA intervals 23h-3h, 7h-15h. The number of rows of this table (1474) is larger than the number of sources (1103) because each radio component of multiple sources is listed as a separate line.
Optical Identifications of B3 Radio Sources (37{deg}..Dec..47{deg}) Name Name of source number=1 The IAU name is given in the name column. This was not given in the B3 Catalogue, and was obtained from the B3 position (hours, minutes, degrees, and tenths of degrees) adding a letter (a, b, etc.) in order of right ascension, in case of ambiguity. Note that this designation does not always match the new VLA position, although this happens rarely. In the case of physically connected multiple sources, a single name is given if they correspond to a single source in the B3 Catalogue; however, some sources listed separately in B3 happen to be parts of the same source (e.g. 0050+401, 0050+403, and 0050+402B) and in this case they retain their individual B3 names. --- Oname 3C or 4C name of source number=2 The othername column gives the 4C name. If the source is also in the 3CR Catalogue, the 3CR name is given instead. 3CR names are recognizable by the format (integer number, or at most one decimal digit), while 4C names are in the DD.NN format. Identification with a 4C source is sometimes ambiguous, as discussed in the B3 Catalogue. --- Sample Number of B3 sample which contained source number=3 This column indicates the source parent subsample. This number indicates inclusion in the sample as originally selected; for example, the physical double 0218+399(A+B) is listed as 0218+399A 1 0218+399B 2 since the respective B3 flux densities are 0.36 and 0.49 Jy, and the components were originally selected as parts of two different samples. The VLA map showed them to be part of the same source; consequently the total 408 MHz flux density is now listed as 0.85 Jy (S408 column) and in any subsequent analysis the source will be considered part of sample 3, 0.8..S..1.6 Jy. Another example is given by the following double source 0218+402(A+B); only one component (A) was originally included in sample 2 (although both components are separately listed in B3) since component B did not meet the selection criteria as given in the published paper. See the paper for full details. --- RAh Right Ascension (B1950) (hour) number=4 These columns give the B1950 position of the source (or component). When no source component was detected with the VLA, the f_S1465 column is marked with an '-' and the given position is from B3 (Ficarra et al. 1985A&AS...59..255F). h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=4 These columns give the B1950 position of the source (or component). When no source component was detected with the VLA, the f_S1465 column is marked with an '-' and the given position is from B3 (Ficarra et al. 1985A&AS...59..255F). --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec f_S1465 Flagged if flux is integrated or upper limit number=5 The f_S1465 column is marked with a "+" if the source (component) was resolved, and an integrated flux density is given. A '-' in the f_S1465 column indicates that the source component was not detected with the VLA and the given flux is an upper limit. For these sources, the listed position is from B3. The S1465 columns gives the source (or component) flux density at 1465 MHz in mJy. --- S1465 Flux density at 1465 MHz in mJy number=5 The f_S1465 column is marked with a "+" if the source (component) was resolved, and an integrated flux density is given. A '-' in the f_S1465 column indicates that the source component was not detected with the VLA and the given flux is an upper limit. For these sources, the listed position is from B3. The S1465 columns gives the source (or component) flux density at 1465 MHz in mJy. mJy MType Morphological classification of source number=6 This column gives a simple morphological classification of the radio structure, as follows: U unresolved, the synthesized beam is not appreciably broadened. R resolved, only one emission peak is present, but the source map or 'response' is wider than the antenna beam. D double source, two emission peaks are present and they appear to be physically related. T triple source, three peaks present and possibly related. The morphological classification is followed by the source's largest angular size (LAS), measured in arcseconds. U implies an (average) upper limit of 5 arcsec; R sources were given a size by measuring the largest HPBW, and deconvolving it with the antenna beam; for D and T sources the separation between the (outermost) components is given. --- S408 Flux density at 408 MHz in Jy number=7 This column gives the total 408 MHz flux density in Jy; generally it is taken from B3, but for extended, strong sources it has been remeasured integrating from the B3 map on the structure revealed by the VLA data. Jy Sp+Index Spectral index between 1465 and 408 MHz number=8 This column gives the spectral index, computed between 1465 and 408 MHz. For multiple sources, the 1465 MHz flux densities have been added. Alpha is defined in the sense S {prop.to} nu^(alpha)^. --- ID Proposed source identification (type) number=9 This column gives the proposed optical identification, as follows: G galaxy B starlike, blue object N starlike object of neutral color Note that the optical identification for multiple sources (e.g. type D or T) is ONLY given for the FIRST listed component, and omitted for all others. A question mark indicates an uncertain optical classification, it does *not* necessarily indicate an uncertain identification. An asterisk preceding the optical classification indicates that the identification was accepted even if it does not meet a uniform criterion of positional agreement (see the paper for details). Note that this column is three characters, with the optical identification being the second character. Thus, to search for all galaxies, one must search for all sources with a 'G' in this column --- f_z '*' if redshift is from the literature number=10 For galaxies, the redshift is given in the z column. If a spectroscopic redshift is available in the literature, the f_z column is marked with an asterisk (*). In this case the reference given in the ref column is to the redshift measurement. To estimate redshifts for those not available in the literature, the image size was measured and from it the redshift was inferred, following an established procedure for radio galaxies (Sandage (1972ApJ...178...25S); Grueff and Vigotti 1979A&AS...35..371G). The method has been recalibrated using spectroscopic redshifts available for 33 radio galaxies in our sample. Some of these are available in the literature, and many were measured by Kron (1986) as an optical follow-up of this program. --- z Estimated or measured redshift number=10 For galaxies, the redshift is given in the z column. If a spectroscopic redshift is available in the literature, the f_z column is marked with an asterisk (*). In this case the reference given in the ref column is to the redshift measurement. To estimate redshifts for those not available in the literature, the image size was measured and from it the redshift was inferred, following an established procedure for radio galaxies (Sandage (1972ApJ...178...25S); Grueff and Vigotti 1979A&AS...35..371G). The method has been recalibrated using spectroscopic redshifts available for 33 radio galaxies in our sample. Some of these are available in the literature, and many were measured by Kron (1986) as an optical follow-up of this program. --- Rmag Red magnitude number=11 For N and B objects, the red magnitude is given, except for some B objects, whose spectroscopic redshift from the literature is given. mag RAoh Optical position Right Ascension (B1950)(hour) h RAom Optical position Right Ascension (B1950)(min) min RAos Optical position Right Ascension (B1950)(sec) s DEo- Optical position Declination sign (B1950) number=12 Right ascension and declination of the optical object. --- DEod Optical position Declination (B1950) (deg) deg DEom Optical position Declination (B1950) (arcmin) arcmin DEos Optical position Declination (B1950) (arcsec) arcsec oRA Radio-optical RA offset number=13 These columns give the radio-minus-optical coordinates differences, in arcsec. arcsec oDE Radio-optical Dec offset number=13 These columns give the radio-minus-optical coordinates differences, in arcsec. arcsec pos_flg Flag indicating which radio position was adopted number=14 This column gives a single digit indicating, for multiple sources, the radio position adopted as follows: 1 first component 2 second component 3 third component 4 unweighted average position (midpoint) 5 weighted average position (radio centroid) --- r_ID Reference code number=15 This column gives a reference code number. For sources with a measured redshift, only the reference for the redshift is given; for 3CR sources, the reader is referred also to Spinrad et al. (1985PASP...97..932S). --- References code reference code --- reftxt reference text --- Patricio Ortiz CDS 1999 Mar 30 UNKNOWN UNKNOWN "The catalogue was originally archived as A016 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_AJ_98_419.xml A 1.4 GHz source survey in an area without nearby rich galaxy clusters J/AJ/99/1071 J/AJ/99/1071 1.4 GHz source survey A 1.4 GHz source survey in an area without nearby rich galaxy clusters J J Condon J M Dickey E E Salpeter Astron. J. 99 1071 1990 1990AJ.....99.1071C Galaxies, radio Radio sources Clusters, globular Photometry, CCD We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z<0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z>0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.
Center of fields and sensitivity of VLA fields Field Field number --- RAh Right Ascension B1950 of field center (hours) h RAm Right Ascension B1950 of field center (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 of field center (sign) --- DEd Declination B1950 of field center (degrees) deg DEm Declination B1950 of field center (minutes) arcmin Srms RMS noise flux density mJy Sneg Flux level for "negative" detections mJy Smin Minimum flux level adopted for detection mJy Radio sources detected by the VLA. Source Source name --- n_Source Note on Source number=1 ? : slightly suspect detections ' : Smax < 2(PBC)Smin --- Field Field whose center is closest to the source --- n_Field Note on Field number=2 * : the source is fairly close to the center of a second field --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Smax Peak flux at 1.4GHz mJy Sint Area integrated flux at 1.4GHz mJy PBC Primary-beam correction factor number=3 PBC(t)=exp[10.7t^2^ + 25.3t^4^] where t is the distance from the source to the field center in degrees. --- Large optical galaxies from POSS plates Gno Galaxy source Number --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec R65%diam Diameter on red plate at level 65% number=1 the levels are defined from the transmission density. Diameters are in microns (1um = 0.067") from the POSS plates 1st epoch um R30%diam Diameter on red plate at level 30% number=1 the levels are defined from the transmission density. Diameters are in microns (1um = 0.067") from the POSS plates 1st epoch um B65%diam Diameter on blue plate at level 65% number=1 the levels are defined from the transmission density. Diameters are in microns (1um = 0.067") from the POSS plates 1st epoch um B30%diam Diameter on blue plate at level 30% number=1 the levels are defined from the transmission density. Diameters are in microns (1um = 0.067") from the POSS plates 1st epoch um mZw Zwicky magnitude of galaxy mag Optical objects coincident with radio sources Source Source name, as in table2 --- u_Source Uncertainty flag --- Otype optical Galaxy or faint object number=1 'G' indicates a coincidence with a galaxy; when this galaxy was optically identified in table3, its number is listed in the last column. These coincidences are listed in table4a of the publication. 'g' indicates a coincidence with an optical faint or unresolved objet, originally listed in table4b of the publication. --- Smax Peak flux at 1.4GHz mJy RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec R65%diam Diameter on red plate at level 65% number=2 the levels are defined from the transmission density. Diameters are in microns (1um = 0.067") from the POSS plates 1st epoch um R30%diam Diameter on red plate at level 30% number=2 the levels are defined from the transmission density. Diameters are in microns (1um = 0.067") from the POSS plates 1st epoch um B65%diam Diameter on blue plate at level 65% number=2 the levels are defined from the transmission density. Diameters are in microns (1um = 0.067") from the POSS plates 1st epoch um B30%diam Diameter on blue plate at level 30% number=2 the levels are defined from the transmission density. Diameters are in microns (1um = 0.067") from the POSS plates 1st epoch um Sep Separation between optical and radio sources arcsec Gno Number in table3 number=1 'G' indicates a coincidence with a galaxy; when this galaxy was optically identified in table3, its number is listed in the last column. These coincidences are listed in table4a of the publication. 'g' indicates a coincidence with an optical faint or unresolved objet, originally listed in table4b of the publication. --- Marie-Jose Wagner, Patricia Bauer, Francois Ochsenbein CDS 1998 Oct 28 We thank Heinz Andernach for supplying the tables 1, 3 and 4. UNKNOWN UNKNOWN * 14-Nov-1997: table2 prepared via OCR at CDS. * 14-Dec-1997: an error in R120 declination was detected by H. Andernach <heinz@polaris.astro.ugto.mx> and corrected. * 28-Oct-1998: tables 1,3,4 prepared by H. Andernach (catalogue numbered R187 in his list) were added. * 03-Nov-1998: an error in table3 (Gno 115 was labelled Gno 117) was detected by Fabienne Woelfel and corrected J_AJ_99_1071.xml BVRI CCD photometry of the metal-poor globular cluster M68 (NGC 4590) J/AJ/99/1831 J/AJ/99/1831 M 68 BVRI photometry BVRI CCD photometry of the metal-poor globular cluster M68 (NGC 4590) G Alcaino W Liller F Alvarado E Wenderoth Astron. J. 99 1831 1990 1990AJ.....99.1831A Clusters, globular Photometry, CCD We present BVRI photometry of the low metallicity globular cluster M68 (NGC 4590) observed with a CCD camera and the 2.2m telescope at ESO/La Silla, and have compared our BV color-magnitude diagrams with the observational results of a previous research. At magnitudes V<22, our BV results, obtained using the INVENTORY code, are in very close agreement with those of the other authors who used DAOPHOT in their reductions. At fainter levels, selection effects appear to affect INVENTORY more than DAOPHOT. We find that V_TO-HB_=3.42+/-0.10, in accord with values found for other clusters. The comparison between our four-color observations and the theoretical isochrones consistently yield a cluster age of 13Gyr with a likely external uncertainty of 2 or 3Gyr. Our derived values for the interstellar reddening at longer wavelengths are generally in agreement (+/-0.02mag) with what would be expected assuming E(B-V)=0.07mag and (m-M)_V_=15.25.
M 68 NGC 4590 12 39 27.9 -26 44 35
CCD magnitudes and colors for 685 stars in NGC 4590 Star Star number -- Saw Sawyer Hogg name (1973PDDO....3....6S) --- Xpos X position number=2 1 pix = 0.36 arcsec. The origin of (X, Y) coordinates is located at the bottom right. pix Ypos Y position number=2 1 pix = 0.36 arcsec. The origin of (X, Y) coordinates is located at the bottom right. pix Vmag V magnitude mag B-V B-V colour index mag V-R V-R colour index mag R-I R-I colour index mag V-I V-I colour index mag B-I B-I colour index mag Marie-Jose Wagner, Patricia Bauer CDS 1997 May 16 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AJ_99_1831.xml The main-sequence turnoff of the old SMC globular cluster NGC 121 J/ApJ/298/544 J/ApJ/298/544 NGC 121 BR photometry The main-sequence turnoff of the old SMC globular cluster NGC 121 L L Stryker G S Da Costa J R Mould Astrophys. J. 298 544 1985 1985ApJ...298..544S Clusters, globular Magellanic Clouds Photometry, CCD globular clusters: general Magellanic Clouds stars: abundances stars: evolution The age of the SMC globular cluster NGC 121 is found from main-sequence isochrone fitting to be 12+/-2x10^9^yr if a distance modulus that assumes Mv=+0.6 for the field RR Lyrae variables near the cluster is used. If instead (m-M)o = 19.3, then the cluster age is 9+/-2x10^9^yr. The cluster is known to contain both RR Lyrae variables and a marginal carbon star; comparison with theoretical models indicates no significant inconsistencies in this joint occurrence at either modulus. The color-magnitude diagram for the nearby field also shows a faint, blue main-sequence turnoff and, in contrast to previous Magellanic Cloud field studies, the field lacks any evidence for the existence of a significant intermediate-age component. A new look at the chemical evolution of the Small Magellanic Cloud suggests that, unlike the Galaxy, where the rate of enrichment has been steady after the initial phase, the enrichment in the SMC remained small for a long interval before increasing rapidly sometime in the last 1-2x10^9^yr.
NGC 121 00 26.7 -71 31
Photometry in NGC 121 Photometry in field Star Star identification number --- B-R B-R color index mag Rmag R magnitude mag Xpos X position number=1 Origin: southwest corner of fig. 1 pix Ypos Y position number=1 Origin: southwest corner of fig. 1 pix DB-R November 18-20 B-R color index difference mag DRmag November 18-20 R magnitude difference mag Marie-Jose Wagner, Patricia Bauer CDS 1996 Sep 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_298_544.xml UBVR CCD photometry of stars in M 31. I. Baade's field IV J/ApJ/324/172 J/ApJ/324/172 M31 UBVR photometry UBVR CCD photometry of stars in M 31. I. Baade's field IV P Hodge M G Lee M Mateo Astrophys. J. 324 172 1988 1988ApJ...324..172H Galaxies, photometry Photometry, CCD galaxies: individual (M 31) galaxies: luminosity function, mass function galaxies: photometry galaxies: stellar content We report deep UBVR CCD photometry of stars in a portion of an arm of M 31, 20kpc southwest of the nucleus. The color-magnitude diagram shows a main sequence that reaches from Mv=-0.7 (at our photometric limit) to Mv=-6.2 and a well-populated giant region. The R, B-R diagram separates the stars rather clearly into three groups, the main sequence, intermediate-color stars (which include the brighter foreground stars), and the red giants. Reddening is found to average E(B-V)=0.13+/-0.04. To determine a reliable luminosity function, we have eliminated foreground contamination and have evaluated our sample completeness, using a large number of artificial stars in the DAOPHOT reduction routine. The corrected luminosity function, which extends from Mv=-5 to -1, has a logarithmic slope of 0.57+/-0.07 for all stars and 0.53+/-0.06 for main-sequence stars only. This value is similar to that reported for galaxies in general (Freedman 1985ApJ...299...74F and 1986, IAUS 116, 61).
M 31 NGC 224 00 42.7 +41 16
Results of UBVR CCD photometry Star Star number --- Xpos X position number=1 Increasing left to right, bottom to top, in Fig. 2. pix Ypos Y position number=1 Increasing left to right, bottom to top, in Fig. 2. pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V color index mag e_B-V rms uncertainty on B-V mag U-B U-B color index mag e_U-B rms uncertainty on U-B mag V-R V-R color index mag e_V-R rms uncertainty on V-R mag Marie-Jose Wagner, Patricia Bauer CDS 1996 Sep 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_324_172.xml The Einstein Observatory survey of stars in the Hyades cluster region. J/ApJ/325/798 J/ApJ/325/798 Einstein survey of stars in the Hyades The Einstein Observatory survey of stars in the Hyades cluster region. G Micela S Sciortino G S Vaiana J H M M Schmitt R A Stern F R Harnden Jr. R Rosner Astrophys. J. 325 798 1988 1988ApJ...325..798M J/ApJ/315/687 : X-Ray emission from solar-type stars: F and G J/ApJ/348/253 : Einstein Survey of Late-type Giant and Supergiant Stars J/ApJ/348/557 : Einstein Survey of the Pleiades Cluster J/ApJ/351/492 : X-ray Emission in the Ursa Major Stream Blanco, V.M., Demers, S., Douglass, G.C., and Fitzgerald, M.P. 1970, U.S. Naval Observatory Photoelectric Catalog (USNO Pub., Vol. 21). Buscombe, W. 1977, MK Spectral Classifications. Third General Catalogue (Evans ton: Northwestern University). Buscombe, W. 1980, MK Spectral Classifications. Fourth General Catalogue (Evanston: Northwestern University). Buscombe, W. 1981, MK Spectral Classifications. Fifth General Catalogue (Evanston: Northwestern University). Cowley, A., et al. 1969, A.J., 141, 83. Gichas, H., Burnham, R., Jr., and Thomas, N. 1962, Lowell Obs. Bull., 5, 257. Gyllenberg, W. 1931, Medd. Lund. Astr. Obs., Ser. II, No. 57 Harnden,, F.R., Jr., Fabricant, D.G., Harris, D.E., and Schwarz, J. 1984, Smithsonian Ap. Obs. Spec. Rept., No. 393. Hoffleit, D. and Jasheck, C. 1982, The Bright Star Catalogue (New Haven: Yale University Observatory). Cat. <V/50> Hoffleit, D., Saladiga, M., and Wlansk, P. 1984, A Supplement to the Bright Star Catalogue (New Haven: Yale University Observatory). Cat. <V/36> Holmberg, E. 1944, Lund. Medd., Ser. II, No. 113. Hertzsprung, E. 1947, Leiden Ann., 19, Pt. 1A. Kapteyn, J.C. and de Sitter, W. 1904, Pub. Kapteyn Astr. Lab. Groningen, No 14. Luyten, W.J., Hill, G., and Morris, S. 1981, Proper Motion Survey With The 48-I nch Schmidt Telescope. LIX. A Catalogue of 929 Possible Candidates for Hyades Membership (Minneapolis: University of Minnesota). Murray, C.A., Lowne, C.M., and Clements, E.D. 1966, Roy. Obs. Bull., No. 108. Osvald, V.V. 1954, Astr. Nach., 281, 193. Pesch, P. 1968, Ap.J., 151, 605. Ramberg, J.M. 1941, Stockhold Ann., 13, No. 9. Stern, R.A., Underwood, J.M., and Antiochos, S.C. 1983, in Second Workshop on Cool Stars Stellar System and the Sun, ed. M.S. Giampapa and L. Golub, Smithsonian Ap. Obs. Spec. Rept. No. 392), Vol. 2, p. 101. van Bueren, H.G. 1952, Bull. Astr. Inst. Netherlands, 11, 385. van Rhijn, P.J. and Raymond, J.J 1934, Pub. Kapteyn Astr. Lab. Groningen, No. 35. Clusters, open Stars, emission X-ray sources open clusters and assocations: individual (Hyades) X-rays: stars The paper reports the results of an extensive X-ray study of the Hyades region and improves on previous studies by using refined X-ray source detection algorithms and the complete set of Einstein Observatory IPC exposures covering the Hyades cluster region (a total of 63 1 x 1 deg images). Maximum likelihood integral X-ray luminosity functions were computed for the Hyades stars for given color index (B-V) ranges. The present results agree substantially with a previous survey about the ubiquity of the stellar activity in the Hyades cluster, especially among solar-type stars. The result of Stern et al. (1981ApJ...249..647S) that stellar X-ray emission is dependent on stellar age is confirmed.
Einstein
EO Survey of Hyades Region: Observation Parameters Seqno Sequence number number=1 The first column gives the IPC sequence number, a two to five digit number which uniquely identifies the observation. The numbers were assigned sequentially at the time of proposal submission. The 'f_Seqno' is flagged with an "a" if the data has been merged from data acquired at epochs spanning months. It is blank otherwise. --- f_Seqno "a" indicates data is merged number=1 The first column gives the IPC sequence number, a two to five digit number which uniquely identifies the observation. The numbers were assigned sequentially at the time of proposal submission. The 'f_Seqno' is flagged with an "a" if the data has been merged from data acquired at epochs spanning months. It is blank otherwise. --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec StartDate Start of observation number=2 The start and stop date of the observation are given in these columns in the form: month-day-year. "MMM:DD:YYYY" StopDate End of observation number=2 The start and stop date of the observation are given in these columns in the form: month-day-year. "MMM:DD:YYYY" livetime Live time of observation number=3 This column gives the observation livetime, in kiloseconds. The livetime is the effective exposure time, a measure of the total time the detectors were able to gather data. It excludes intervals lost because of Earth occultation, because of passage through the South Atlantic Anomaly, or because of unacceptable aspect solution. The livetime has been corrected for detector dead time, a fractional correction for the time during which the detector is unable to record events because it is "processing" a prior event. ks EO Survey of Hyades Stars: Optical Properties and X-ray Luminosities Name Star name number=1 This column lists the star name. We use the following naming conventions. EG -- Eggen and Greenstein (1965ApJ...141...83E, 1965ApJ...142..925E) GH -- Gichas, et al. (1962) GY -- Gyllenberg (1931) H -- Hanson (1975AJ.....80..379H) Ho -- Holmberg (1944) Hz -- Hertzsprung (1947) HTK -- Luyten as quoted by Herbig (1962) HZ -- Humason and Zwicky (1947ApJ...105...85H) J -- Johnson, et al. (1962ApJ...136...75J) KA -- Kapteyn and de Sitter (1904) L -- Pels, et al. (1975A&A....43..423P) LP -- Luyten, et al. (1981) MLC -- Murray, et al. (1966) O -- Osvald (1954) Ra -- Ramberg (1941) VA -- van Altena (1969AJ.....74....2V) VB -- van Bueren (1952) VR -- van Rhijn and Raymond (1934) VYS -- Vyssotsky (1956AJ.....61..201V) WOR -- Worley (1962AJ.....67..396W) --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Vmag Apparent visual magnitude number=2 These columns give the apparent visual magnitude, the B-V color, and the reference for mv and/or B-V. mag B-V B-V color index number=2 These columns give the apparent visual magnitude, the B-V color, and the reference for mv and/or B-V. mag r_B-V Reference for mv and/or B-V number=2 These columns give the apparent visual magnitude, the B-V color, and the reference for mv and/or B-V. --- Sp Spectral type number=3 These columns give the spectral type and the reference for the spectral type. This is a comma separated list, an asterisk '*' indicates that Spectral types computed from Color Index or rotational velocity inferred from modulation of chromospheric emission. --- r_Sp Reference for spectral type, comma separated number=3 These columns give the spectral type and the reference for the spectral type. This is a comma separated list, an asterisk '*' indicates that Spectral types computed from Color Index or rotational velocity inferred from modulation of chromospheric emission. --- Vsini Equatorial (rotational) velocities along line of sight (more than one value) number=4 These columns give the equatorial rotational velocity, projected along the line of sight, and the reference for the rotational velocity. km/s r_Vsini Reference for vsini. comma separated list number=4 These columns give the equatorial rotational velocity, projected along the line of sight, and the reference for the rotational velocity. --- Notes Notes --- status "A" if Certainty about Hyades membership; "B" if "Potential" number=9 The "status" column lists an "A" if the star is one of the 121 "Certain" Hyades members, or a "B" if the star is one of 10 "Potential" Hyades members whose Hyades membership has been rejected by Hanson (1975AJ.....80..379H). --- VName Star name (first name found in Name) number=1 This column lists the star name. We use the following naming conventions. EG -- Eggen and Greenstein (1965ApJ...141...83E, 1965ApJ...142..925E) GH -- Gichas, et al. (1962) GY -- Gyllenberg (1931) H -- Hanson (1975AJ.....80..379H) Ho -- Holmberg (1944) Hz -- Hertzsprung (1947) HTK -- Luyten as quoted by Herbig (1962) HZ -- Humason and Zwicky (1947ApJ...105...85H) J -- Johnson, et al. (1962ApJ...136...75J) KA -- Kapteyn and de Sitter (1904) L -- Pels, et al. (1975A&A....43..423P) LP -- Luyten, et al. (1981) MLC -- Murray, et al. (1966) O -- Osvald (1954) Ra -- Ramberg (1941) VA -- van Altena (1969AJ.....74....2V) VB -- van Bueren (1952) VR -- van Rhijn and Raymond (1934) VYS -- Vyssotsky (1956AJ.....61..201V) WOR -- Worley (1962AJ.....67..396W) --- f_Lx Flagged "1" if Lx is an upper limit number=5 This column is flagged with a "1" if the X-ray luminosity is an upper limit. Upper limits given are 3-sigma upper bounds for all members of the optical sample that fall within 2' of the position of an object from the Einstein Observatory master catalog (which includes ~60 different catalogs) and Herbig and Rao (1972ApJ...174..401H). --- Lx X-ray luminosity from 0.16-4.0 keV number=6 The X-ray luminosity from 0.16-4.0 keV is presented in the "Lx" column and the corresponding statistical uncertainties in the "e_Lx" column (one sigma). If the luminosity is an upper limit, the uncertainty is listed as 0.000. The conversion factor from count rate to luminosity, assuming a common distance of 45 parsecs (Hanson 1975AJ.....80..379H) for all cluster members, is 4.860 *10^30^ ergs/count. The estimated overall error in the X-ray luminosities is a factor of ~2 and consists of statistical errors (less than 40% for the 2.5 sigma sources), systematic errors in instrument calibrations (<~10%, Harnden, et al. 1984), errors due to the individual cluster member distance (<100%), and systematic errors in converting count to flux due to the assumed source temperature (<~40%). 10-7W e_Lx Error for luminosity number=6 The X-ray luminosity from 0.16-4.0 keV is presented in the "Lx" column and the corresponding statistical uncertainties in the "e_Lx" column (one sigma). If the luminosity is an upper limit, the uncertainty is listed as 0.000. The conversion factor from count rate to luminosity, assuming a common distance of 45 parsecs (Hanson 1975AJ.....80..379H) for all cluster members, is 4.860 *10^30^ ergs/count. The estimated overall error in the X-ray luminosities is a factor of ~2 and consists of statistical errors (less than 40% for the 2.5 sigma sources), systematic errors in instrument calibrations (<~10%, Harnden, et al. 1984), errors due to the individual cluster member distance (<100%), and systematic errors in converting count to flux due to the assumed source temperature (<~40%). 10-7W flux_flg Flag indicating how flux was evaluated number=7 This column indicates how the flux was calculated. We use the following abbreviations: MB = from "Map" cell count rate, increased by 25% LC = from "Local" count rate in a 3'-radius circle LB = from "Local" cell count rate, increased by 25% WM = weighted mean for source observed more than once Count rates were increased by 25% before their conversion to flux when they were partially obscured and detected with the "map" method or when they were detected only with the "map" method. They were also increased by 25% for upper limits. See the appendices of the paper for complete details. --- reco Ribs and Edge Code flag number=8 This column is flagged "Y" if the X-ray luminosity is derived in the presence of potential source shadowing. Reco is a ribs and edge code, indicating that the source fell on or near the detector ribs or edges. The local detect algorithm uses a detection cell subdivided into nine central subcells (3x3) with a background frame (around the central cell) subdivided into 16 subcells. The 'reco' value provides an estimate of the number of background and detection subcells potentially obscured and is nonzero whenever a source could have any of its central or frame subcells obscured. However, this approach necessarily employs simplifying assumptions regarding the shape and dimensions of the ribs, and it neglects spectral dependencies. Consequently, although a quantitative attempt is made to correct for such effects, the only completely reliable approach is to regard count rates for sources with nonzero reco values (flagged "Y" here) as indeterminate. See appendix A of the paper for more details. --- References code reference code --- reftxt bibcode (if any) and reference text --- Patricio Ortiz CDS 1999 Mar 31 UNKNOWN UNKNOWN Prepared from the tables available at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) J_ApJ_325_798.xml Blue straggler stars in the globular cluster NGC 5053 J/ApJ/336/780 J/ApJ/336/780 gr photometry of NGC 5053 blue stragglers Blue straggler stars in the globular cluster NGC 5053 J M Nemec J G Cohen Astrophys. J. 336 780 1989 1989ApJ...336..780N Clusters, globular Photometry Stars, blue binaries: general celestial mechanics, stellar dynamics globular clusters: general stars: evolution Twenty-four blue straggler stars have been identified in the low central concentration globular cluster NGC 5053. New deep color-magnitude (C-M) diagrams to 23mag, constructed from photometry of over 6000 stars on 4-shooter CCD frames, show that they form a well-defined sequence in the C-M diagram, extending up to ~2.2mag brighter than the main-sequence turnoff point. The 12 most luminous blue stragglers are found to be significantly more centrally concentrated than the cluster subgiants with magnitudes in the same interval (a similar result is known for the blue stragglers in the globular cluster NGC 5466). Furthermore, they are also found to be more centrally concentrated than the 12 lower luminosity blue stragglers. Comparisons of the projected radial distributions of the bright and faint blue stragglers, with the radial distributions that are expected for stars of mass 0.8, 1.6, and 2.4M_{sun}_, (calculated using multimass King models) suggests that the brightest blue stragglers have an average mass of <M>=1.3+/0.3M_{sun}_, which is less than or comparable to twice the mean mass of a main-sequence turnoff star, and the lower luminosity blue stragglers have a mean mass similar to that of the main-sequence turnoff stars (i.e., M~0.8M_{sun}_). By fitting theoretical isochrones computed by Bell and VandenBerg to the observed main-sequence turnoff and subgiant branch regions of NGC 5053, a distance modulus of (m-M)_0_=16.05+/-0.14mag, and an age of 18+/-3Gyr are derived for NGC 5053. The main-sequence luminosity function shows no sign of "turning over" for stars brighter than M_g_~5mag. For a description of the uvgr photometric system, see e.g. <GCPD/38>
NGC 5053 13 16 26.9 +17 41 52
Photometry of the brightest stars in fields 1, 2, 3 and 4 Field Field designation number=1 A = Field 1, B = Field 2, C = Field 3, D = Field 4 --- Seq Sequential number in the field --- Xpos X position number=2 1 pix = 0.33", X increasing to the North, Y increasing to the West. pix Ypos Y position number=2 1 pix = 0.33", X increasing to the North, Y increasing to the West. pix gmag g magnitude mag g-r g-r colour index mag Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 29 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_336_780.xml The Nonthermal Stellar Dynamics of the Globular Cluster M15 J/ApJ/347/251 J/ApJ/347/251 Dynamics of Globular Cluster M15 The Nonthermal Stellar Dynamics of the Globular Cluster M15 R C Peterson P Seitzer K M Cudworth Astrophys. J. 347 251 1989 1989ApJ...347..251P J/AJ/106/154 : HST Observations in inner region of M15 (Ferraro+ 1993) J/AJ/107/1745 : HST UVI photometry of M5. II. (Yanny+, 1994) J/AJ/107/2067 : Fabry-Perot measurements of M15 (Gebhardt+, 1994) J/AJ/110/704 : RR Lyrae in M15 (Silbermann+ 1995) Kustner F., 1921, Veroff. Sternw. Bonn, No 15 =1921VeUSB..15....1K Clusters, globular Radial velocities celestial mechanics, stellar dynamics globular clusters: general techniques: radial velocities The velocity dispersion as a function of radius in the globular cluster M15 is derived from measurements of 120 individual stars between 0.1' and 4.6' of the cluster center, and from the integrated light of the central cusp. The stellar measurements, with an individual accuracy of 1 km/s, indicate a mean cluster velocity of -107.1+/-0.9 km/s, and a mean velocity dispersion of 9.0+/-0.6 km/s. The velocity dispersion inside 1' varies with radius. The dispersion of the 27 stars within 20" is 14.2+/-1.9 km/s, while that of the 30 stars between 0.5' and 1.2' is 8.4+/-1.4 km/s. The cusp itself appears to have a dispersion of at least 25 km/s. Except for its greater velocity broadening, the spectrum of the integrated light of the cusp is indistinguishable from that formed by superposition of the individual M15 giant spectra, demonstrating that the excess light at the center is due primarily to the normal M15 population. The increase of the dispersion toward the center is not consistent with truncated isothermal (King-Michie) models, for which the velocity dispersion is nearly constant within a few core radii and then falls steeply beyond. The observed behaviour is difficult to reconcile as well with current post-core collapse models, which are also isothermal and whose central energy sources are modest. It is indicative of a nonthermal energy distribution with substantial heating in the central regions; this is consistent with a central black hole of about 1000 M_{sun}_.
Velocities for M15 members JD-2440000 Julian date (-2440000) of each observation Mean Julian date of each observation, except for stars observed more than once, where the date of the first observation is listed. d RAh Right ascension (equinox 1950.0) Equatorial coordinates are as measured by Cudworth, except that AC [Auriere & Cordoni 1981, A&AS, 46, 347] coordinates were used for their stars 271, 417, 456, 457, 488, 576, 623, 780, and 787. h RAm R.A. min RAs R.A. s DE- Declination sign (always blank) --- DEd Declination (equinox 1950.0) deg DEm Dec. arcmin DEs Dec. arcsec Dist Radial distance from cluster center Radius and position angle from the point marked by the large cross in Figure 1 of the printed paper, RA = 21h 27m 33.33s, DE=+11d 56m 48.8s arcmin PA Position angle positive north through east deg RV Measured radial velocity For all multiply-observed stars, this is the weighted mean of the N independent observations in Table 2, except for K912, where the velocity and uncertainty were derived from the single spectrum formed by coadding the two separate exposures. km/s e_RV Internal uncertainty in RV km/s Vmag V magnitude V magnitude, from preliminary measurements by Cudworth except for stars inside 0.35', where AC values are used. mag Kustner Number from Kustner (1921VeUSB..15....1K) --- Other Other star name Other star name: Auriere & Cordoni (1981A&AS...46..347A) prefix AC; Sandage (1970ApJ...162..841S) prefix S; Arp (1955AJ.....60..317A) Roman numeral prefix. --- Stars with multiple velocity measurements JD-2440000 Julian date (-2440000) d RV Measured radial velocity km/s e_RV Internal uncertainty in RV km/s Kustner Number from Kustner (1921VeUSB..15....1K) --- Other Other star name Other star name: Auriere & Cordoni (1981A&AS...46..347A) prefix AC; Arp (1955AJ.....60..317A) Roman numeral prefix. --- Velocities for M15 nonmembers JD-2440000 Julian date (-2440000) of each observation d RAh Right ascension (equinox 1950.0) h RAm R.A. min RAs R.A. s DE- Declination sign (always blank) --- DEd Declination (equinox 1950.0) deg DEm Dec. arcmin DEs Dec. arcsec RV Measured radial velocity km/s e_RV Internal uncertainty in RV km/s Vmag V magnitude mag Kustner Number from Kustner (1921VeUSB..15....1K) --- CDS 1995 Jul 11 AAS CD-ROM series, Volume 4 1995 Lee Brotzman [ADS] 06-May-1995 J_ApJ_347_251.xml EINSTEIN Observatory magnitude-limited X-ray survey of late-type giant and supergiant stars. J/ApJ/348/253 J/ApJ/348/253 Late type giants and supergiants in X-Ray EINSTEIN Observatory magnitude-limited X-ray survey of late-type giant and supergiant stars. A Maggio G S Vaiana B M Haisch R A Stern J Bookbinder F R Harnden Jr. R Rosner Astrophys. J. 348 253 1990 1990ApJ...348..253M J/ApJ/315/687 : X-Ray emission from solar-type stars: F and G J/ApJ/325/798 : Einstein Survey of Hyades-cluster Region J/ApJ/348/557 : Einstein Survey of the Pleiades Cluster J/ApJ/351/492 : X-ray Emission in the Ursa Major Stream Stars, atmospheres Stars, giant Stars, supergiant X-ray sources stars: stars: coronae X-rays: general X-rays: stars Results are presented of an extensive X-ray survey of 380 giant and supergiant stars of spectral types from F to M, carried out with the Einstein Observatory. It was found that the observed F giants or subgiants (slightly evolved stars with a mass M less than about 2 solar masses) are X-ray emitters at the same level of main-sequence stars of similar spectral type. The G giants show a range of emission more than 3 orders of magnitude wide; some single G giants exist with X-ray luminosities comparable to RS CVn systems, while some nearby large G giants have upper limits on the X-ray emission below typical solar values. The K giants have an observed X-ray emission level significantly lower than F and F giants. None of the 29 M giants were detected, except for one spectroscopic binary.
Einstein
EO Survey of Late-type Giant and Supergiant Stars HR HR (Bright Star Catalog) number number=1 These columns give the HR (Bright Star Catalog) number, the HD (Henry Draper Catalog) number, and other name of the star. A single five or six digit number in the "Name" column indicates the SAO Catalog number. --- HD HD (Henry Draper Catalog) number number=1 These columns give the HR (Bright Star Catalog) number, the HD (Henry Draper Catalog) number, and other name of the star. A single five or six digit number in the "Name" column indicates the SAO Catalog number. --- Name Other name number=1 These columns give the HR (Bright Star Catalog) number, the HD (Henry Draper Catalog) number, and other name of the star. A single five or six digit number in the "Name" column indicates the SAO Catalog number. --- Sp Spectral Type number=2 These columns give the spectral type and optical class of the star. A "G" in the "class" column indicates that the star is a Giant (luminosity classes III-IV, II, and II-III). An "S" in the "class" column indicates that the star is a Supergiant (luminosity classes II, II-I, and I). --- class Giant/Supergiant Luminosity Class number=2 These columns give the spectral type and optical class of the star. A "G" in the "class" column indicates that the star is a Giant (luminosity classes III-IV, II, and II-III). An "S" in the "class" column indicates that the star is a Supergiant (luminosity classes II, II-I, and I). --- B-V B-V color index number=3 These columns give optical information about the star; the B-V color index, apparent visual magnitude, and absolute magnitude are listed. Unknown values are set to 99.9 mag Vmag Visual magnitude (apparent) number=3 These columns give optical information about the star; the B-V color index, apparent visual magnitude, and absolute magnitude are listed. Unknown values are set to 99.9 mag Mabs Absolute magnitude number=3 These columns give optical information about the star; the B-V color index, apparent visual magnitude, and absolute magnitude are listed. Unknown values are set to 99.9 mag plx Trigonometric Parallax number=4 This column gives the trigonometric parallax, in arcseconds. Unknown values are set to 99.99 arcsec mult Single/Multiple System Classification number=5 The "mult" column classifies a source as single ("S"), multiple ("M"), or RS CVn-like ("R"). An asterisk ("*") flags the star (in the "f_Vmag" column) as having mv < 6.3. The importance of careful discrimination between single stars and multi-component systems is clear if one wants to use the luminosity or rotational velocity with confidence. It is possible that more of the objects may belong in the RS CVn category, but further observations are needed to confirm this. We have classified a system as multiple if one of the following is indicated: (a) confirmed or suspected spectroscopic binaries (88 objects), (b) stars with either a physical or visual companion nearer than 2' (56 objects), because of the photon collecting area we used (see Maggio, et al. 1990ApJ...348..253M for details), (c) stars with variable radial velocity, unless a companion is known at more than 2' (32 objects), (d) 10 more objects with three or more components for which we cannot judge the distance of the nearest companion. --- f_Vmag "*" indicates star with Vmag < 6.3 number=5 The "mult" column classifies a source as single ("S"), multiple ("M"), or RS CVn-like ("R"). An asterisk ("*") flags the star (in the "f_Vmag" column) as having mv < 6.3. The importance of careful discrimination between single stars and multi-component systems is clear if one wants to use the luminosity or rotational velocity with confidence. It is possible that more of the objects may belong in the RS CVn category, but further observations are needed to confirm this. We have classified a system as multiple if one of the following is indicated: (a) confirmed or suspected spectroscopic binaries (88 objects), (b) stars with either a physical or visual companion nearer than 2' (56 objects), because of the photon collecting area we used (see Maggio, et al. 1990ApJ...348..253M for details), (c) stars with variable radial velocity, unless a companion is known at more than 2' (32 objects), (d) 10 more objects with three or more components for which we cannot judge the distance of the nearest companion. --- Seqno IPC sequence number number=6 The "Seqno" column gives the Einstein sequence number, a two to five digit number which uniquely identifies the observation. The numbers were assigned at the time of proposal submission. --- obscode Observer code number=7 The observer listed in this column is the observer code from the "Yellow Book" (Seward and Martenis), the corresponding names are listed below. Observer Code Observers ------------- --------- S Serendipitous CfA stellar survey 0 Harvard-Smithsonian Center for Astrophysics stellar team 1 Columbia Astrophysical Laboratory 2 MIT 3 Goddard Space Flight Center 34 J. Nelson and F. Cordova, U. of California, Berkeley 54 C. Bowyer, F. Walter, and P. Charles, U. of California, Berkeley 97 R. Stern, J. Underwood, and S. Antiochos, JPL 99 C. Zwaan, A. Brinkman, and R. Mewe, Sonnenborgh Obs. 128 T. Ayres, B. Haisch, and J. Linsky, U. of Colorado 179 T. Snow and W. Cash, U. of Colorado 208 J. Linsky and T. Ayres, U. of Colorado 222 C. Bowyer and F. Walter, U. of California, Berkeley 227 H. Zirin, Hale Observatory 254 J. Linsky, R. Stencel, and G. Basri, U. of Colorado 255 G. Wallerstein and L. Willson, U. of Washington 265 D. Gibson, New Mexico Tech 288 S. Catalano, C. Blanco, E. Marilli, G. Peres, and S. Serio, U. of Catania 322 H. Johnson, Lockheed Research Laboratory 341 B. Haisch and T. Simon, Lockheed Research Laboratory 381 L. Hartmann and A. Dupree, Harvard College Obs. 385 C. Zwaan, A. Boggende, A. Brinkman, and R. Mewe, Sonnenborgh Observatory 398 A. Michalitsianos, M. Kafatos, and R. Hobbs, Goddard Space Flight Center 427 G. Riegler, R. Stern, and J. Underwood, JPL 445 C. Bowyer, F. Walter, and P. Charles, U. of California, Berkeley 449 T. Simon, R. Stencel, M. Giampapa, and J. Linsky, U. of Colorado 480 C. Bowyer, B. Bopp, and F. Walter, U. of California, Berkeley 501 E. Bohm-Vitense and S. Parson, U. of Heidmann, NRAO-VA 519 R. Stern, J. Underwood, and S. Antiochos, JPL 626 T. Simon and R. Stencel, U. of Colorado 994 H. Johnson, Lockheed Research Laboratory --- nobs Number of observations number=8 The "nobs" column lists the total number of observations for each star. In the case of multiple observations we quote, for conciseness, only the sequence with the longest exposure time. --- f_fx "1" if flux is an upper limit number=9 These columns are marked with a one ("1") if the quantities which follow (the X-ray flux density, the log of fx/fv, and the X-ray luminosity) are upper limits. Upper limits given are 3-sigma upper bounds for all members of the optical sample that fall within 2' of the position of an object from the Einstein Observatory master catalog (which includes ~60 different catalogs). Only three multiply-observed stars failed to be detected in each repeated exposure: for these three stars, the derived upper limits are consistent with the X-ray fluxes derived from the detections. --- fx X-ray Flux in the 0.16-4.0 keV band number=10 These columns list the X-ray flux density (* E-13 erg/cm^2^/s) at the Earth and the corresponding statistical errors. X-ray fluxes were computed at Earth in the energy range 0.16-4.0 keV, using a constant conversion factor of 2.0E-11 erg/ct/cm^2^ times the IPC count rate. This value assumes a thermal spectrum (continuum + lines), from a plasma with solar abundances at a temperature log T=6.5. In computing an effective count rate for each source, the standard Rev-1 processing applies corrections, for mirror scattering and vignetting and for the IPC point response, and flags possible shadowing by the support structure of the IPC entrance aperture through the use of a so-called rib and edge code. However, due to a spectral dependence of these corrections (especially the point response correction), they are only approximate for sources whose spectra are dissimilar to those assumed in computing the corrections. Because the detection cell for the broad band is relatively small for the rather soft stellar sources, only ~70% of stellar source counts fall inside the cell, a fraction about 25% smaller than assumed in computing the standard correction factors. Therefore, for local, obscured X-ray detections, and for all map detections, we have increased the standard (corrected) values by this factor of ~25%, and for all local, unobscured X-ray detections we have computed net source counts from a circle of 3' radius centered at the source position and background counts in a concentric annulus width inner and outer radii of 5' and 6'. This same 25% correction has been applied to the upper bounds (which are only evaluated using the local method). When more than one observation was available for a given star, we adopted the following procedure (see Micela, et al. 1988ApJ...325..798M for details): 1. For detections, we computed a weighted (by inverse square of statistical error) mean count rate, preferring unobscured measurements to those for which shadowing was possible. 2. For upper bounds, we selected the lowest unobscured value, if available, and otherwise conservatively retained the largest value. Taking into account a conversion factor error of ~50%, statistical errors of <~40%, and systematic errors in the instrument calibrations of <~10%, we estimate the overall error in the quoted X-ray fluxes to be <~70%. 10-16W/m2 e_fx Error on X-ray Flux number=10 These columns list the X-ray flux density (* E-13 erg/cm^2^/s) at the Earth and the corresponding statistical errors. X-ray fluxes were computed at Earth in the energy range 0.16-4.0 keV, using a constant conversion factor of 2.0E-11 erg/ct/cm^2^ times the IPC count rate. This value assumes a thermal spectrum (continuum + lines), from a plasma with solar abundances at a temperature log T=6.5. In computing an effective count rate for each source, the standard Rev-1 processing applies corrections, for mirror scattering and vignetting and for the IPC point response, and flags possible shadowing by the support structure of the IPC entrance aperture through the use of a so-called rib and edge code. However, due to a spectral dependence of these corrections (especially the point response correction), they are only approximate for sources whose spectra are dissimilar to those assumed in computing the corrections. Because the detection cell for the broad band is relatively small for the rather soft stellar sources, only ~70% of stellar source counts fall inside the cell, a fraction about 25% smaller than assumed in computing the standard correction factors. Therefore, for local, obscured X-ray detections, and for all map detections, we have increased the standard (corrected) values by this factor of ~25%, and for all local, unobscured X-ray detections we have computed net source counts from a circle of 3' radius centered at the source position and background counts in a concentric annulus width inner and outer radii of 5' and 6'. This same 25% correction has been applied to the upper bounds (which are only evaluated using the local method). When more than one observation was available for a given star, we adopted the following procedure (see Micela, et al. 1988ApJ...325..798M for details): 1. For detections, we computed a weighted (by inverse square of statistical error) mean count rate, preferring unobscured measurements to those for which shadowing was possible. 2. For upper bounds, we selected the lowest unobscured value, if available, and otherwise conservatively retained the largest value. Taking into account a conversion factor error of ~50%, statistical errors of <~40%, and systematic errors in the instrument calibrations of <~10%, we estimate the overall error in the quoted X-ray fluxes to be <~70%. 10-16W/m2 f_fx/fv "1" if fx/fv is an upper limit number=9 These columns are marked with a one ("1") if the quantities which follow (the X-ray flux density, the log of fx/fv, and the X-ray luminosity) are upper limits. Upper limits given are 3-sigma upper bounds for all members of the optical sample that fall within 2' of the position of an object from the Einstein Observatory master catalog (which includes ~60 different catalogs). Only three multiply-observed stars failed to be detected in each repeated exposure: for these three stars, the derived upper limits are consistent with the X-ray fluxes derived from the detections. --- fx/fv log of X-ray to visual flux ratio number=11 This column lists the log of the X-ray to visual flux ratio, computed as log fx/fv = log fx + mv/2.5 + 5.47 This distance- and radius-independent parameter is very useful in our survey because of the large percentage of stars with unknown parallax. --- f_logLx "1" if logLx is an upper limit number=9 These columns are marked with a one ("1") if the quantities which follow (the X-ray flux density, the log of fx/fv, and the X-ray luminosity) are upper limits. Upper limits given are 3-sigma upper bounds for all members of the optical sample that fall within 2' of the position of an object from the Einstein Observatory master catalog (which includes ~60 different catalogs). Only three multiply-observed stars failed to be detected in each repeated exposure: for these three stars, the derived upper limits are consistent with the X-ray fluxes derived from the detections. --- logLx Log of X-ray Lum. in the 0.16-4.0 keV band number=12 This column gives the log of the X-ray luminosity. In the computation of luminosities, a large source of error can be introduced by uncertainties in the individual stellar distances (as much as a factor of 2 or more); for this reason, we have computed X-ray luminosities only for stars with available trigonometric parallaxes greater than 0.01. [10-7W] l_Vsini Upper limit flag to Vsini number=13 These columns list the radial velocity, when available, and the reference from which the radial velocity was taken. Upper limits are denoted by a '<' in the column 'l_Vsini'. The used references are: 1 Hoffleit, D. and Jaschek,C. 1982, The Bright Star Catalogue (New Haven: Yale University Press). (See Cat. <V/50>) 2 Gray, D.F. (1982ApJ...262..682G) 3 Herbig, G. and Spalding, J. (1955ApJ...121..118H) 4 Gray, D.F. and Toner, C.G. (1986ApJ...310..277G) 5 Gray, D.F. and Nagar, P. (1985ApJ...298..756G) --- Vsini Rotational velocity number=13 These columns list the radial velocity, when available, and the reference from which the radial velocity was taken. Upper limits are denoted by a '<' in the column 'l_Vsini'. The used references are: 1 Hoffleit, D. and Jaschek,C. 1982, The Bright Star Catalogue (New Haven: Yale University Press). (See Cat. <V/50>) 2 Gray, D.F. (1982ApJ...262..682G) 3 Herbig, G. and Spalding, J. (1955ApJ...121..118H) 4 Gray, D.F. and Toner, C.G. (1986ApJ...310..277G) 5 Gray, D.F. and Nagar, P. (1985ApJ...298..756G) km/s r_Vsini Reference for rotational velocity number=13 These columns list the radial velocity, when available, and the reference from which the radial velocity was taken. Upper limits are denoted by a '<' in the column 'l_Vsini'. The used references are: 1 Hoffleit, D. and Jaschek,C. 1982, The Bright Star Catalogue (New Haven: Yale University Press). (See Cat. <V/50>) 2 Gray, D.F. (1982ApJ...262..682G) 3 Herbig, G. and Spalding, J. (1955ApJ...121..118H) 4 Gray, D.F. and Toner, C.G. (1986ApJ...310..277G) 5 Gray, D.F. and Nagar, P. (1985ApJ...298..756G) --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Patricio Ortiz CDS 1999 Apr 21 UNKNOWN UNKNOWN Prepared from the tables available at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) J_ApJ_348_253.xml X-ray studies of coeval star samples. II. The Pleiades cluster as observed with the Einstein Observatory. J/ApJ/348/557 J/ApJ/348/557 X-ray studies of stars in the Pleiades X-ray studies of coeval star samples. II. The Pleiades cluster as observed with the Einstein Observatory. G Micela S Sciortino G S Vaiana F R Harnden R Rosner J H M M Schmitt Astrophys. J. 348 557 1990 1990ApJ...348..557M J/ApJ/315/687 : X-Ray emission from solar-type stars: F and G J/ApJ/348/253 : Einstein Survey of Late-type Giant and Supergiant Stars J/ApJ/325/798 : Einstein Survey of Hyades-cluster Region J/ApJ/351/492 : X-ray Emission in the Ursa Major Stream Ahmed, F., Lawrence, L., and Reddish, V.C. 1965, Pub. Roy. Obs. Edinburgh, Vol. 1, No. 7. Hertzsprung, E. 1947, Ann. Leiden Obs., Vol. 19, Pt. 1A. McCarthy, M.F. and Treanor, P.S. 1964, Ric. Astr., 6, 535. Seward, F.D. and Martenis, P. 1986, Einstein Observatory Catalog of Observations (the "Yellow Book"; 5th ed.; Cambridge: Harvard-Smithsonian Center for Astrophysics). van Leeuween, F. 1983, Ph.D. thesis, Leiden. Clusters, open Stars, emission X-ray sources open clusters and associations: individual (Pleiades) stars: rotation stars: X-rays Coronal X-ray emission of the Pleiades stars is investigated, and maximum likelihood, integral X-ray luminosity functions are computed for Pleiades members in selected color-index ranges. A detailed search is conducted for long-term variability in the X-ray emission of those stars observed more than once. An overall comparison of the survey results with those of previous surveys confirms the ubiquity of X-ray emission in the Pleiades cluster stars and its higher rate of emission with respect to older stars. It is found that the X-ray emission from dA and early dF stars cannot be proven to be dissimilar to that of Hyades and field stars of the same spectral type. The Pleiades cluster members show a real rise of the X-ray luminosity from dA stars to early dF stars. X-ray emission for the young, solar-like Pleiades stars is about two orders of magnitude more intense than for the nearby solar-like stars.
Einstein
EO Survey of the Pleiades: Optical Properties and X-ray Luminosities Name Star name number=1 This column gives the star name(s), coded according to the following conventions: A: Asiago observatory flare stars ALR: Ahmed, Lawrence and Reddish (1965) B: Byurakan observatory flare stars Hz: Hertzsprung (1947) JRS: Stauffer (1984ApJ...280..189S) MT: McCarthy and Treanor (1964) (1964RA......6..535M) P: Pels (Quoted in van Leeuween, 1983) van Leeuween, F. 1983, Ph.D. thesis, Leiden. T: Tonantzintla flare stars (Cat.<II/131>) VM: VanMaanen (1945ApJ...102...26V) --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Vmag Apparent Visual magnitude number=2 These columns give the following optical properties of the stars: the apparent visual magnitude, the B-V color index, the spectral type, and the equatorial (rotational) velocity projected along the line of sight. Optical properties are taken from the literature (see references below). If a the spectral property or rotational velocity is not known, a '...' appears as the entry in the column. mag r_Vmag Reference for visual magnitude number=3 These columns list the reference used to obtain Vmag, Sp, and Vsini. --- B-V B-V color index number=2 These columns give the following optical properties of the stars: the apparent visual magnitude, the B-V color index, the spectral type, and the equatorial (rotational) velocity projected along the line of sight. Optical properties are taken from the literature (see references below). If a the spectral property or rotational velocity is not known, a '...' appears as the entry in the column. mag Sp Spectral type number=2 These columns give the following optical properties of the stars: the apparent visual magnitude, the B-V color index, the spectral type, and the equatorial (rotational) velocity projected along the line of sight. Optical properties are taken from the literature (see references below). If a the spectral property or rotational velocity is not known, a '...' appears as the entry in the column. --- r_Sp Reference for spectral type number=3 These columns list the reference used to obtain Vmag, Sp, and Vsini. --- Vsini Equatorial (rotational) velocities along line of sight number=2 These columns give the following optical properties of the stars: the apparent visual magnitude, the B-V color index, the spectral type, and the equatorial (rotational) velocity projected along the line of sight. Optical properties are taken from the literature (see references below). If a the spectral property or rotational velocity is not known, a '...' appears as the entry in the column. km/s r_Vsini Reference for vsini Comma separated list number=3 These columns list the reference used to obtain Vmag, Sp, and Vsini. --- notes Notes on the source number=4 This column is for notes on the source. In particular, we have noted when we believe a star is variable (var.) or binary (bin). If there is no note on the source, a '...' appears as the entry in the column. --- f_Lx "1" if luminosity is an upper limit number=5 The "f_Lx" column is flagged with a "1" if the X-ray luminosity is an upper limit. Upper limits given are 3-sigma upper bounds for all members of the optical sample that fall within 2' of the position of an object from the Einstein Observatory master catalog (which includes ~60 different catalogs). The log of the X-ray luminosity from 0.16-4.0 keV is presented in the "lx" column and the corresponding error (by percentage) is listed in the "e_lx" column. If the luminosity is an upper limit, the uncertainty is listed as 0.000. --- Lx log of X-ray luminosity from 0.16-4.0 keV number=5 The "f_Lx" column is flagged with a "1" if the X-ray luminosity is an upper limit. Upper limits given are 3-sigma upper bounds for all members of the optical sample that fall within 2' of the position of an object from the Einstein Observatory master catalog (which includes ~60 different catalogs). The log of the X-ray luminosity from 0.16-4.0 keV is presented in the "lx" column and the corresponding error (by percentage) is listed in the "e_lx" column. If the luminosity is an upper limit, the uncertainty is listed as 0.000. [10-7W] e_Lx Percentage-error on X-ray luminosity number=5 The "f_Lx" column is flagged with a "1" if the X-ray luminosity is an upper limit. Upper limits given are 3-sigma upper bounds for all members of the optical sample that fall within 2' of the position of an object from the Einstein Observatory master catalog (which includes ~60 different catalogs). The log of the X-ray luminosity from 0.16-4.0 keV is presented in the "lx" column and the corresponding error (by percentage) is listed in the "e_lx" column. If the luminosity is an upper limit, the uncertainty is listed as 0.000. % flx_flg Flag indicating how flux was evaluated number=6 This column indicates how the X-ray flux is evaluated: MB: from the "Map" cell count rate LB: from the "Local" cell count rate WM: from a weighted mean, for sources observed more than once See the paper (1990ApJ...348..557M) for further details. --- reco Ribs and Edge Code flag number=7 This column is flagged "Y" if the X-ray luminosity is derived in the presence of potential source shadowing. Reco is a ribs and edge code, indicating that the source fell on or near the detector ribs or edges. The local detect algorithm uses a detection cell subdivided into nine central subcells (3x3) with a background frame (around the central cell) subdivided into 16 subcells. The reco value provides an estimate of the number of background and detection subcells potentially obscured and is nonzero whenever a source could have any of its central or frame subcells obscured. However, this approach necessarily employs simplifying assumptions regarding the shape and dimensions of the ribs, and it neglects spectral dependencies. Consequently, although a quantitative attempt is made to correct for such effects, the only completely reliable approach is to regard count rates for sources with nonzero reco values (flagged "Y" here) as indeterminate. See the paper (1990ApJ...348..557M) for more details. --- EO Survey of the Pleiades: Observation Parameters Seqno Sequence Number number=1 This column gives the Einstein "sequence" number of the field. The sequence number is a two to five digit number which uniquely identifies the observation. The numbers were assigned sequentially at the time of proposal submission. --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Date Observation Date number=2 These columns give the date of the observation and the original obs of the field. The obs listed is from the "Yellow Book" (Seward and Martenis, 1986). --- live Live Time number=3 This column gives the observation live time, in kiloseconds. The live time is the effective exposure time, a measure of the total time the detectors were able to gather data. It excludes intervals lost because of Earth occultation, because of passage through the South Atlantic Anomaly, or because of unacceptable aspect solution. The livetime has been corrected for detector dead time, a fractional correction for the time during which the detector is unable to record events because it is "processing" a prior event. ks Obs Original Einstein Observer number=2 These columns give the date of the observation and the original obs of the field. The obs listed is from the "Yellow Book" (Seward and Martenis, 1986). --- Files with references code reference code --- reftxt reference text --- Patricio Ortiz CDS 1999 Mar 31 UNKNOWN UNKNOWN Prepared from the tables available at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) J_ApJ_348_557.xml Luminous asymptotic giant branch stars in the Large Magellanic Cloud J/ApJ/348/98 J/ApJ/348/98 LMC AGB stars IRAS fluxes Luminous asymptotic giant branch stars in the Large Magellanic Cloud N Reid C Tinney J Mould Astrophys. J. 348 98 1990 1990ApJ...348...98R Infrared sources Magellanic Clouds Stars, giant galaxies: stellar content infrared: sources Magellanic Clouds stars: evolution stars: late-type stars: variables: other (long-period variables) We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_<9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_<-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.
IRAS
TRM selected sources in LMC north TRM TRM designation number=1 TRM (1990ApJ...348...98R) selected sources in the LMC north field. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Scan Information on the scan directions number=2 Information on the scan directions in which each source was detected unambiguously is given. 1: detected in EW scan 2: detected in NS scan 3: detected in both EW and NS scans --- S12 Flux density at 12 {mu}m number=3 Fluxes listed in this table assume a flux distribution which varies as {nu}-1 (see Sec. IV). Blank entries in the S12, S25, S60, or S100 columns imply either that no flux was detected at that wavelength, or that the region was so confused that the source extraction algorithm was unable to extract any flux, or that the flux density measurement is not reliable. Jy S25 Flux density at 25 {mu}m number=3 Fluxes listed in this table assume a flux distribution which varies as {nu}-1 (see Sec. IV). Blank entries in the S12, S25, S60, or S100 columns imply either that no flux was detected at that wavelength, or that the region was so confused that the source extraction algorithm was unable to extract any flux, or that the flux density measurement is not reliable. Jy S60 Flux density at 60 {mu}m number=3 Fluxes listed in this table assume a flux distribution which varies as {nu}-1 (see Sec. IV). Blank entries in the S12, S25, S60, or S100 columns imply either that no flux was detected at that wavelength, or that the region was so confused that the source extraction algorithm was unable to extract any flux, or that the flux density measurement is not reliable. Jy S100 Flux density at 100 {mu}m number=3 Fluxes listed in this table assume a flux distribution which varies as {nu}-1 (see Sec. IV). Blank entries in the S12, S25, S60, or S100 columns imply either that no flux was detected at that wavelength, or that the region was so confused that the source extraction algorithm was unable to extract any flux, or that the flux density measurement is not reliable. Jy PSC See note number=4 Sources marked with a "*" have been associated positionally with an object in the IRAS PSC --- Rej Rejection (Y: yes, N: no) --- Com Comments on rejection number=6 S100: Source was rejected because it had S100>S60>2S25. S60 Source was rejected because it had S60>2S25. S25>> S12 Source was rejected because it had S25>4S12. GC, C, NSO: Source was rejected because it coincided with a globular cluster, open cluster, or clearly nonstellar object on the V or I band Schmidt plates. PN: Source was rejected because it coincided with a planetary nebula (Sanduleak refs). H{alpha}: Source coincided with a knot of Half in the LMC emission-line survey of Davies et al. (1976MmRAS..81...89D) (c), (u): Source extraction algorithm was unable to produce a meaningful flux estimate at that wavelength, due to either (c) source confusion or (u) unselected source; however, it is clear from the IRAS maps that there is sufficient 60 {mu}m or 100 {mu}m flux present to reject the source. 1: TRM 147 showed some weak evidence fro 60 {mu}m flux which was not selected by IPAC source extractor. Since this source had a PSC 60 {mu}m flux greater than its 25 {mu}m flux, it was therefore rejected. The flux conditions were held to be stronger reasons for source rejection, so although a number of sources listed as being rejected on this basis were also coincident positionally with globular clusters, galaxies, etc., only the flux conditions has been listed here. --- Patricia Bauer CDS 1996 Sep 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_348_98.xml X-ray studies of coeval star samples. III. X-ray emission in the Ursa Major stream. J/ApJ/351/492 J/ApJ/351/492 X-ray emission in the Ursa Major stream. X-ray studies of coeval star samples. III. X-ray emission in the Ursa Major stream. J H M M Schmitt G Micela S Sciortino G S Vaiana F R Harnden R Rosner Astrophys. J. 351 492 1990 1990ApJ...351..492S J/ApJ/315/687 X-Ray emission from solar-type stars : F and G J/ApJ/348/253 Einstein Survey of Late-type Giant and Supergiant Stars J/ApJ/325/798 Einstein Survey of Hyades-cluster Region J/ApJ/348/557 Einstein Survey of the Pleiades Cluster Harnden, F.R., Jr., Fabricant, D.G., Harris, D.E., and Schwarz, J. 1984, Smithsonian Ap. Obs. Spec. Rept., No. 393. Clusters, open Stars, emission X-ray sources open clusters and associations: general stars: rotation X-rays: stars Results are reported from a comprehensive survey of X-ray emission from stars known or suspected to be members of the UMa cluster and/or stream. Of the 42 UMa member stars surveyed, 18 were detected as X-ray sources, and spectral analysis was performed for 10 stars with sufficient X-ray counts. Consideration is given to relations between X-ray luminosity, color, and kinematics of the sample stars, and the X-ray spectra of the UMa stars are discussed in the context of the general problem of stellar X-ray temperatures. Also confirmed is the lack of X-ray-emitting A dwarfs among UMa members; among stars of later spectral type there is a rather large dispersion in X-ray luminosity. This dispersion cannot readily be explained by contamination with field star interlopers and appears rather to be a property of the UMa X-ray luminosity distribution function.
Einstein
X-ray Emssion in the Ursa Major Stream: X-ray Results and Optical Properties HR HR (Bright Star Catalog) number number=1 These columns give the HR (Bright Star Catalog) and HD (Henry Draper Catalog) numbers of the sample star. --- HD HD (Henry Draper Catalog) number number=1 These columns give the HR (Bright Star Catalog) and HD (Henry Draper Catalog) numbers of the sample star. --- inst Instrument number=2 These columns give the instrument used and the sequence number of the observation. Listed in the instrument column will be an "I" if the Imaging Proportional Counter (IPC) was used, an "H" if the High Resolution Imager (HRI) was used, or an "EXO" if the data is from EXOSAT. The Einstein sequence number is a two to five digit number which uniquely identifies the observation. The numbers were assigned sequentially at the time of proposal submission. In most cases we used IPC data, for a few stars the HRI was used, and in one case the EXOSAT Low Energy experiment was used. --- Seqno Sequence Number number=2 These columns give the instrument used and the sequence number of the observation. Listed in the instrument column will be an "I" if the Imaging Proportional Counter (IPC) was used, an "H" if the High Resolution Imager (HRI) was used, or an "EXO" if the data is from EXOSAT. The Einstein sequence number is a two to five digit number which uniquely identifies the observation. The numbers were assigned sequentially at the time of proposal submission. In most cases we used IPC data, for a few stars the HRI was used, and in one case the EXOSAT Low Energy experiment was used. --- f_CCR Flagged "1" if count rate is an upper limit number=3 The "f_CCR" column is marked with a "1" if the corrected count rate is an upper limit. The "CCR" column gives the corrected count rate (per 1000 seconds). For detections, the "f_CCR" column is marked with a "0", and the 1 sigma error is given in the "e_CCR" column. For upper limits, the value given is a 3 sigma upper limit, and the error is given as zero. Count rate is corrected for scattering, vignetting, and detector dead time. --- CCR Corrected Count Rate number=3 The "f_CCR" column is marked with a "1" if the corrected count rate is an upper limit. The "CCR" column gives the corrected count rate (per 1000 seconds). For detections, the "f_CCR" column is marked with a "0", and the 1 sigma error is given in the "e_CCR" column. For upper limits, the value given is a 3 sigma upper limit, and the error is given as zero. Count rate is corrected for scattering, vignetting, and detector dead time. ct/ks e_CCR Error on count rate number=3 The "f_CCR" column is marked with a "1" if the corrected count rate is an upper limit. The "CCR" column gives the corrected count rate (per 1000 seconds). For detections, the "f_CCR" column is marked with a "0", and the 1 sigma error is given in the "e_CCR" column. For upper limits, the value given is a 3 sigma upper limit, and the error is given as zero. Count rate is corrected for scattering, vignetting, and detector dead time. ct/ks method Detect method number=4 This column marks what kind of detect algorithm was used to locate the source; an "M" indicates MDETECT, an "L" indicates LDETECT (see Harnden, et al. 1984). This pertains only to the IPC data. Sources detected with other detectors contain a "." in this column. --- logLx Log of X-ray luminosity from 0.16-4.0 keV number=5 This column gives the log of the X-ray luminosity (in erg/s) in the 0.16-4.0 keV passband, computed with the distance given in the table st_uma_2.dat . When the count rate is an upper limit, the luminosity is also an upper limit. For the conversion from count rate to fluxes, we used the "standard" conversion of 2x10^-11^ erg/cm^2^/count. [10-7W] note Notes on the source number=6 This column contains notes on individual sources. The following notes are used: a: HR 1971: observed with Ribs and Edges COde (RECO; see text) 1008 b: HR 5328/29: not separated by IPC; observed with RECO 200 c: HR 5727/28: not separated by IPC d: HR 8207: observed with RECO 1006 e: HR 8410: observed with RECO 400 --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Dist Distance to star number=7 In these columns, we give the adopted distance, the B-V color index, and the spectral type. pc B-V B-V color index number=7 In these columns, we give the adopted distance, the B-V color index, and the spectral type. mag Sp Spectral type number=7 In these columns, we give the adopted distance, the B-V color index, and the spectral type. --- U U velocity number=8 The space velocities, U, V, and W are given (in km/s) in the first three columns listed here. Note that we are using a coordinate system with the positive U-axis pointing toward the Galactic center. In the "Rho" column, we give the modulus of the velocity difference between the star and the cluster nucleus adopted from Eggen (1983AJ.....88..642E) to be U(nuc)= 13.9 km/s, V(nuc)= 1.5 km/s, and W(nuc)= -9.4 km/s. km/s V V velocity number=8 The space velocities, U, V, and W are given (in km/s) in the first three columns listed here. Note that we are using a coordinate system with the positive U-axis pointing toward the Galactic center. In the "Rho" column, we give the modulus of the velocity difference between the star and the cluster nucleus adopted from Eggen (1983AJ.....88..642E) to be U(nuc)= 13.9 km/s, V(nuc)= 1.5 km/s, and W(nuc)= -9.4 km/s. km/s W W velocity number=8 The space velocities, U, V, and W are given (in km/s) in the first three columns listed here. Note that we are using a coordinate system with the positive U-axis pointing toward the Galactic center. In the "Rho" column, we give the modulus of the velocity difference between the star and the cluster nucleus adopted from Eggen (1983AJ.....88..642E) to be U(nuc)= 13.9 km/s, V(nuc)= 1.5 km/s, and W(nuc)= -9.4 km/s. km/s Rho Velocity number=8 The space velocities, U, V, and W are given (in km/s) in the first three columns listed here. Note that we are using a coordinate system with the positive U-axis pointing toward the Galactic center. In the "Rho" column, we give the modulus of the velocity difference between the star and the cluster nucleus adopted from Eggen (1983AJ.....88..642E) to be U(nuc)= 13.9 km/s, V(nuc)= 1.5 km/s, and W(nuc)= -9.4 km/s. km/s X-ray Emission in the Ursa Major Stream: Temperature Fits HD HD (Henry Draper Catalog) number number=1 The HD (Henry Draper Catalog) number of the sample star is given in this column. --- Seqno Sequence number number=2 This column gives the Einstein sequence number, a two to five digit number which uniquely identifies the observation. Sequence numbers were assigned sequentially at the time of proposal submission. --- ntemps Number of temperature components in fit number=3 This column gives the number of temperature components which were used in the spectral analysis. --- logT1 log T for low-temperature component number=4 These columns give the best-fit single temperature for each component (logT1 and logT2), along with the one sigma (68% confidence) errors. For fits which had only one component, the second component entries will be zero. [K] e_logT1 Downward 68% confidence error number=4 These columns give the best-fit single temperature for each component (logT1 and logT2), along with the one sigma (68% confidence) errors. For fits which had only one component, the second component entries will be zero. [K] E_logT1 Upward 68% confidence error number=4 These columns give the best-fit single temperature for each component (logT1 and logT2), along with the one sigma (68% confidence) errors. For fits which had only one component, the second component entries will be zero. [K] logT2 log T for high-temperature component number=4 These columns give the best-fit single temperature for each component (logT1 and logT2), along with the one sigma (68% confidence) errors. For fits which had only one component, the second component entries will be zero. [K] e_logT2 Downward 68% confidence error number=4 These columns give the best-fit single temperature for each component (logT1 and logT2), along with the one sigma (68% confidence) errors. For fits which had only one component, the second component entries will be zero. [K] E_logT2 Upward 68% confidence error number=4 These columns give the best-fit single temperature for each component (logT1 and logT2), along with the one sigma (68% confidence) errors. For fits which had only one component, the second component entries will be zero. [K] chi2 Reduced chi-square number=5 This column gives the reduced chi-squared of the temperature fit. --- em1d2 Emission measure number=6 These columns give the derived emission measure (in units of 10^49^ cm^-3^ pc^-2^) of the best-fit spectrum. For fits which had only one component, the entry for the second component will be zero. 10+49/cm3/pc2 em2d2 Emission measure number=6 These columns give the derived emission measure (in units of 10^49^ cm^-3^ pc^-2^) of the best-fit spectrum. For fits which had only one component, the entry for the second component will be zero. 10+49/cm3/pc2 logLx1 log X-ray luminosity from 0.16-4.0 keV number=7 These columns give the log of the inferred X-ray luminosity (with the distance as given in st_uma_1.dat) in ergs/s in the 0.16-4.0 keV passband. For fits which had only one component, the entry for the second component will be zero [10-7W] logLx2 log X-ray luminosity from 0.16-4.0 keV number=7 These columns give the log of the inferred X-ray luminosity (with the distance as given in st_uma_1.dat) in ergs/s in the 0.16-4.0 keV passband. For fits which had only one component, the entry for the second component will be zero [10-7W] Patricio Ortiz CDS 1999 Apr 07 UNKNOWN UNKNOWN Prepared from the tables available at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) J_ApJ_351_492.xml A deep Abell cluster redshift survey J/ApJ/365/66 J/ApJ/365/66 Redshifts of a sample of distant Abell gal. clusters A deep Abell cluster redshift survey J P Huchra J P Henry M Postman M J Geller Astrophys. J. 365 66 1990 1990ApJ...365...66H galaxies: clusters: general galaxies: distances and redshifts We have measured redshifts for a complete sample of 145 Abell clusters of galaxies. The sample covers a 561 square degree region at high Galactic latitude. The median redshift of the clusters in the sample is 0.16. For R >= 1 clusters the correlation length is r_0_ = 21 h^-1^ Mpc. The amplitude of the correlation function is a factor of 1.4 less than that obtained by Bahcall and Soneira, but the difference is within the 1 {sigma} uncertainties. In this sample we cannot detect clustering on scales >~ 70 h^-1^ Mpc. Although the maps of the cluster distribution in redshift space show a large void of diameter ~20,000 km s^-1^, frequent occurrence of such large empty regions is consistent with the smaller scale behaviour of the correlation function of the survey. Large-scale peculiar motions are <~1000 km s^-1^. This limit is inconsistent with the claim of detection by Bahcall, Soneira, and Burgett of ~2000 km/s peculiar motions. We suggest that the earlier result is affected by the Corona Borealis supercluster, which contributes more than a third of the excess pairs in the shallower survey. Notes: Some errors have been corrected. See notes of "table2".
Mean redshift of Abell clusters CluID A for "Abell" added at CDS for clarity --- Anumb number in the Abell catalogue --- RAh Right ascension (B1950) of the cluster centre (hours) h RAm right ascension (minutes) min DE- declination sign (B1950) --- DEd declination of the cluster center (degrees) (B1950) deg DEm declination (minutes) arcmin R Abell's richness class --- D Abell's distance class --- m1 brightness of 1st-ranked galaxy from Leir & vandenBergh 1977, ApJS 34, 381 (1),(2) mag m10 brightness of 10th-ranked galaxy (1),(2) mag Zest estimated redshift --- Zobs observed redshift --- Ngal number of galaxies with measured z --- Ref reference code(s), see --- NOTE notes --- Redshifts of individual galaxies Name name of object, either in format hhmm+ddmm appended by A or B for close pairs of galaxies, or N.... for an NGC number --- RAh Right ascension (B1950) of galaxy h RAm Right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign (B1950) . DEd declination (B1950) of galaxy (degrees) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec Zobs observed redshift --- Vhel heliocentric radial velocity km/s Verr heliocentric radial velocity error km/s Ref reference code(s), see number=3 Reference codes: CFH = Ciardullo, Ford and Harms 1985, ApJ 293, 69 DJ = Jenner 1974, ApJ 191, 55 F = Fetisova 1982 SvA 25, 647 HGT = Hoessel, Gunn and Thuan 1980, ApJ 241, 486 HH+ = Hintzen, et al. 1982, AJ 87, 1656 HSM = Hintzen, Scott and McKee 1980, ApJ 242, 857 JH = This paper, Mt. Hopkins data, ApJ 365, 66 OWT = Owen, White, & Thronson 1988, AJ 95, 1 PH = This paper, Mauna Kea data, ApJ 365, 66 RK = Rhee and Katgert 1988, A&AS 72, 243 SGH = Schneider, Gunn, and Hoessel 1983, ApJ 264, 337 SRS = Sarazin, Rood and Struble 1982, A&A 108, L7 --- Abell Abell name 'Annnn' or 'Annnn/m', the latter stands for 'Annnn or Annnm' (5) number=6 In some cases the galaxy is associated with two galaxy clusters indicated as 'A1283/9 and A1289/3'. Note that the published version incorrectly states A1283/8 and A1289/8. H.A. 7-Mar-94 --- NOTE notes as published --- Heinz Andernach CDS 1994 Mar 04 The files were forwarded to CDS by Heinz J. Andernach (courtesy M. Postman). J_ApJ_365_66.xml New velocity dispersions and photometry for E and S0 galaxies in the great attractor J/ApJ/368/54 J/ApJ/368/54 New velocity dispersions and photometry for New velocity dispersions and photometry for E and S0 galaxies in the great attractor A Dressler S M Faber D Burstein Astrophys. J. 368 54 1991 1991ApJ...368...54D galaxies: distances and redshifts galaxies: internal motions galaxies: photometry *** No Description Available ***
catalogue of velocity, total blue magnitude, photometric diameter, velocity dispersion, and absorption-line index SPS SPS survey number (see paper) --- NAME NGC or IC number --- TYPE morphological type --- GRN group number assigned by the authors (see paper) --- Vh heliocentric velocity determined in this study km/s Vg heliocentric group velocity of each GRN km/s AB B-band Galactic extinction mag BT total blue magnitude mag lgDn log of photometric diameter Dn (0.1arcmin) 0.1arcmin lgSIG log of central velocity dispersion (km/s) km/s Mg2 Mg b absorption line index (see paper) mag Koichi Nakajima CDS 1993 Nov 15 UNKNOWN UNKNOWN The files were forwarded to CDS by Heinz J. Andernach (courtesy D. Burstein) J_ApJ_368_54.xml The luminosity function of compact groups of galaxies J/ApJ/380/30 J/ApJ/380/30 The luminosity function of compact groups of The luminosity function of compact groups of galaxies C Mendes De Oliveira P Hickson Astrophys. J. 380 30 1991 1991ApJ...380...30M galaxies: clusters: general galaxies: interactions galaxies: luminosity function, mass function We present an analysis of the luminosity function of the galaxies in Hickson's sample of compact groups (HCG). The luminosities of compact group galaxies are consistent with their being drawn from a Schechter luminosity function with {alpha} = -2^+0.8^_-0.9_, L* = 1.1 +/- 0.2 x 10^10^ h^-2^ L_Sun_ and PHI* = 1.3^+0.2^_-0.8_ h^3^/Mpc^3^ (99% confidence level). Individual morphological-type luminosity functions were also determined. Both the total and morphological-type specific luminosity functions of compact group galaxies are significantly different form those of field, loose-group, and cluster galaxies. In particular, the luminosity function of HCG elliptical galaxies has a mean magnitude which is significantly brighter than the mean magnitude of Virgo cluster elliptical galaxies. (28% of HCG elliptical galaxies are more luminous than M87). The mean luminosity density of galaxies in compact groups is estimated to be 1.3^+0.1^_0.8_ x 10^6^ h L_Sun_ Mpc^-3^, which constitutes ~0.8% of the total luminosity density of galaxies in the universe. This result is consistent with the conventional scenario in which compact groups merge to form elliptical galaxies on a relatively short time scale.
Absolute magnitudes of HCG galaxies HCG Designation in "Hickson's Compact Groups of galaxies", 1982, ApJ 255, 382 --- MB-5log(h) Absolute magnitude of individual galaxies, h=Ho/100, Ho=Hubble constant mag James Marcout, Francois Ochsenbein CDS 1994 Jul 11 UNKNOWN UNKNOWN Keypunched at CDS J_ApJ_380_30.xml The Rosseland mean free-free Gaunt factor of the dense high-Temperature stellar plasma J/ApJ/382/636 J/ApJ/382/636 Rosseland mean free-free Gaunt factor The Rosseland mean free-free Gaunt factor of the dense high-Temperature stellar plasma N Itoh F Kuwashima K Ichihashi H Mutoh Astrophys. J. 382 636 1991 1991ApJ...382..636I J/ApJS/63/661 : Relativistic Free-Free Gaunt Factor (Nakagawa+ 1987) J/ApJS/74/291 : Relativistic Free-Free Gaunt Factor. II. (Itoh+ 1990) Atomic physics Opacities atomic processes dense matter opacities plasmas The Rosseland mean free-free Gaunt factor of the dense high-temperature stellar plasma is calculated, based on both the accurate relativistic cross section and Sommerfeld's exact nonrelativistic cross section. A wide range of electron degeneracy is accurately taken into account. Comparison of the resulting free-free opacity with the electron conduction opacity is made.
*Results of calculations of <<g^-1^>> Eta Value of the degeneracy parameter, {eta} --- Elem Element for Gaunt factor calculation number=1 The Rosseland mean inverse Gaunt factor was calculated for the following: H - relativistic hydrogen He - relativistic helium C - relativistic carbon O - relativistic oxygen G - exact nonrelativistic inverse Gaunt factor --- G-4.0 Gaunt factor, log({gamma}^2^) = -4.0 --- G-3.5 Gaunt factor, log({gamma}^2^) = -3.5 --- G-3.0 Gaunt factor, log({gamma}^2^) = -3.0 --- G-2.5 Gaunt factor, log({gamma}^2^) = -2.5 --- G-2.0 Gaunt factor, log({gamma}^2^) = -2.0 --- G-1.5 Gaunt factor, log({gamma}^2^) = -1.5 --- G-1.0 Gaunt factor, log({gamma}^2^) = -1.0 --- G-0.5 Gaunt factor, log({gamma}^2^) = -0.5 --- G+0.0 Gaunt factor, log({gamma}^2^) = 0.0 --- G+0.5 Gaunt factor, log({gamma}^2^) = 0.5 --- G+1.0 Gaunt factor, log({gamma}^2^) = 1.0 --- G+2.0 Gaunt factor, log({gamma}^2^) = 2.0 --- CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee E. Brotzman [ADS] 27-Aug-97 J_ApJ_382_636.xml The distribution of nearby rich clusters of galaxies J/ApJ/384/404 J/ApJ/384/404 Redshifts of a sample of nearby rich gal. clusters The distribution of nearby rich clusters of galaxies M Postman J P Huchra M J Geller Astrophys. J. 384 404 1992 galaxies: clusters: general galaxies: distances and redshifts We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC >= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.
catalogue of redshifts of a sample of nearby rich clusters of galaxies CluID Cluster ID: A=Abell, V=Virgo cluster; these codes added at CDS for clarity --- Anumb Abell number, or 0 for Virgo --- RAh Right ascension (B1950) of the cluster centre (hours) h RAm right ascension (minutes) min DE- declination sign (B1950) . DEd declination of the cluster center (degrees) (B1950) deg DEm declination (minutes) arcmin R Abell's richness class --- D Abell's distance class --- m1 brightness of 1st-ranked galaxy from Leir & vandenBergh 1977, ApJS 34, 381 number=1 Note that due to the different origin of the data, m1 can be higher than m10 (e.g. for A1892). Moreover, the magnitude scale for northern clusters (A1-A2712) is different from that for the southern clusters (A>2712). Trailing zeroes in m1, m10 and Zest were truncated at CDS. mag m10 brightness of 10th-ranked galaxy number=1 Note that due to the different origin of the data, m1 can be higher than m10 (e.g. for A1892). Moreover, the magnitude scale for northern clusters (A1-A2712) is different from that for the southern clusters (A>2712). Trailing zeroes in m1, m10 and Zest were truncated at CDS. mag Zest estimated z number=1 Note that due to the different origin of the data, m1 can be higher than m10 (e.g. for A1892). Moreover, the magnitude scale for northern clusters (A1-A2712) is different from that for the southern clusters (A>2712). Trailing zeroes in m1, m10 and Zest were truncated at CDS. --- Zobs observed z --- Ngal number of galaxies with measured z --- r_z reference code(s), see number=2 Reference codes: DS Dressler & Shectman 1988a, AJ 95, 284 and Dressler & Shectman 1988b, AJ 95, 985 F Fetisova 1981, SvA 25, 647 FJ Forman & Jones 1991, priv.comm. GC Chapman, Geller & Huchra 1988, AJ 95, 999 HGT Hoessel, Gunn & Thuan 1980, ApJ 241, 486 HHPG Huchra et al. 1990, ApJ 365, 66 HPGG Huchra, Postman, Geary, Geller 1991, in preparation HSM Hintzen, Scott and McKee 1980, ApJ 242, 857 JH HHPG, Mt. Hopkins observations K Karachentsev & Kopylov 1981, SvALett 7, 285 and Klypin & Kopylov 1983, SvALett 9, 41 and Kopylov, Fetisova & Schvartsman 1984, Astron. Tsirk. 1344, 1 QMIT Quintana et al. 1985, AJ 90, 410 PH HHPG, Mauna Kea observations RK Rhee & Katgert 1988, A&AS 72, 243 SGH Schneider, Gunn & Hoessel 1983, ApJ 264, 377 and Schneider 1982, PhD Thesis, CalTech SHEC Schectman 1985, ApJS 57, 77 SR Struble & Rood 1987, ApJS ApJS 63, 543 SRS Sarazin, Rood & Struble 1982, A&A 108, L7 UL Ulrich 1978, ApJ 221, 422 VCC Vettolani et al. 1989, A&AS 79, 147 VCSZ Vettolani et al. 1990, AJ 99, 1709 ZCAT CfA redshift survey sources ZHG Zabludoff, Huchra & Geller 1990, ApJS 74, 1 and Zabludoff 1992, PhD thesis, in prep. --- NOTE notes number=3 These notes do not appear in the published table, but were kept in the electronic version as received from M. Postman. --- Heinz Andernach CDS 1994 Mar 05 UNKNOWN UNKNOWN The catalogue was provided by courtesy of Marc Postman to Heinz Andernach. It was numbered A133 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" J_ApJ_384_404.xml IRAS observations of young stellar objects in the Corona Australis dark cloud J/ApJ/397/520 J/ApJ/397/520 IRAS observations in Cr A IRAS observations of young stellar objects in the Corona Australis dark cloud B A Wilking P G Thomas C J Lada M R Meyer E T Young Astrophys. J. 397 520 1992 1992ApJ...397..520W Associations, stellar Infrared sources Photometry, infrared infrared: stars ISM: clouds ISM: individual (Corona Australis Cloud) stars: pre-main sequence An analysis of IRAS data is presented for a 57pc^2^ area of the nearby Corona Australis dark cloud complex. A total of 79 far-infrared sources are detected at 12{mu}m or in at least three IRAS bands. Combining these data with both newly obtained and previously published optical/infrared data, a total of 16 IRAS sources are identified with young stellar objects which are in close proximity to the R Coronae Australis cloud or Rossano Cloud B. Among these objects is a cold, heavily obscured young stellar object, IRAS 32, which radiates only in the 25-100{mu}m bands and is found to be associated with an extended near-infrared nebula. The majority of the remaining 63 IRAS sources in the sample appear to be related to field stars.
*IRAS Sources with S(25)/S(12)>0.8. No Source number --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec l_S12 Limit flag on S12 --- S12 Flux density at 12 {mu}m number=1 Flux densities and source sizes followed by a colon are uncertain due to low signal-to-noise and/or source confusion. "c" indicates source confusion which did not permit a flux determination. All flux densities were determined from in-scan slices using the ADDSCAN utility, except for Sources 21 and 34 which were derived from the Pointed Observations Jy u_S12 Uncertainty flag on S12 --- W12 Source size deconvolved with a Gaussian beam of 0.76' (12{mu}m) arcmin u_W12 Uncertainty flag on W12 --- n_W12 p indicates that source size is consistent with point source --- S25 Flux density at 25 {mu}m number=1 Flux densities and source sizes followed by a colon are uncertain due to low signal-to-noise and/or source confusion. "c" indicates source confusion which did not permit a flux determination. All flux densities were determined from in-scan slices using the ADDSCAN utility, except for Sources 21 and 34 which were derived from the Pointed Observations Jy u_S25 Uncertainty flag on S25 --- W25 Source size deconvolved with a Gaussian beam of 0.77' (25{mu}m) arcmin u_W25 Uncertainty flag on W25 --- n_W25 p indicates that source size is consistent with point source --- l_S60 Limit flag on S60 --- S60 Flux density at 60 {mu}m number=1 Flux densities and source sizes followed by a colon are uncertain due to low signal-to-noise and/or source confusion. "c" indicates source confusion which did not permit a flux determination. All flux densities were determined from in-scan slices using the ADDSCAN utility, except for Sources 21 and 34 which were derived from the Pointed Observations Jy u_S60 Uncertainty flag on S60 --- W60 Source size deconvolved with a Gaussian beam of 1.39' (60{mu}m) arcmin n_W60 p indicates that source size is consistent with point source --- l_S100 Limit flag on S100 --- S100 Flux density at 100 {mu}m number=1 Flux densities and source sizes followed by a colon are uncertain due to low signal-to-noise and/or source confusion. "c" indicates source confusion which did not permit a flux determination. All flux densities were determined from in-scan slices using the ADDSCAN utility, except for Sources 21 and 34 which were derived from the Pointed Observations Jy u_S100 Uncertainty flag on S100 --- n_S100 c indicates source confusion --- W100 Source size deconvolved with a Gaussian beam of 2.96' (100{mu}m) arcmin u_W100 Uncertainty flag on W100 --- n_W100 p indicates that source size is consistent with point source --- Star Visible stars? number=2 "TT" denotes T Tauri star. References to spectral types and H{alpha} emission from Knacke et al. 1973 and Marraco & Rydgren 1981. --- Notes Associations, notes number=3 (1) Near-infrared photometry for 2{mu}m sources presented in Table 3 (2) Extended emission associated with visible reflection nebula. (3) Source is badly confused in all bands. Integrated fluxes are greater than 60Jy at 60 mum and greater than 240Jy at 100{mu}m. (4) S CrA is a double with separation of 1.4 (Herbig 1962). (5) Far-infrared source also mapped by Cruz-Gonzales, McBreen, & Fazio 1984 and/or Wilking et al. 1985. (6) TS 13.1, R1, and R2 are from the 2{mu}m survey of Taylor & Storey 1984. (7) The HH100-IR source is confused with R CrA. Flux densities for both sources were derived assuming R CrA is a point source in all bands. (8) VV CrA is a double star with separation of 2" with companion brightest in the infrared (B. Reipurth 1991, private comm.). (9) VSS 10 is from the 2 mum survey of Vrba, Strom, & Strom 1976a. (10) Source associated with Cloud B (Rossano 1978). --- *IRAS Sources with S(25)/S(12)<0.8. No Source number --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec S12 Flux density at 12 {mu}m number=1 Flux densities and source sizes followed by a colon are uncertain due to low signal-to-noise and/or source confusion. "c" indicates where source confusion did not permit a flux determination. All flux densities were determined from in-scan slices using the ADDSCAN. Upper limits are 3 times the rms noise. Except where noted in col. "Notes", all in-scan sources sizes are consistent with point sources. Jy u_S12 Uncertainty flag on S12 --- l_S25 Limit flag on S25 --- S25 Flux density at 25 {mu}m number=1 Flux densities and source sizes followed by a colon are uncertain due to low signal-to-noise and/or source confusion. "c" indicates where source confusion did not permit a flux determination. All flux densities were determined from in-scan slices using the ADDSCAN. Upper limits are 3 times the rms noise. Except where noted in col. "Notes", all in-scan sources sizes are consistent with point sources. Jy u_S25 Uncertainty flag on S25 --- l_S60 Limit flag on S60 --- S60 Flux density at 60 {mu}m number=1 Flux densities and source sizes followed by a colon are uncertain due to low signal-to-noise and/or source confusion. "c" indicates where source confusion did not permit a flux determination. All flux densities were determined from in-scan slices using the ADDSCAN. Upper limits are 3 times the rms noise. Except where noted in col. "Notes", all in-scan sources sizes are consistent with point sources. Jy l_S100 Limit flag on S100 --- S100 Flux density at 100 {mu}m number=1 Flux densities and source sizes followed by a colon are uncertain due to low signal-to-noise and/or source confusion. "c" indicates where source confusion did not permit a flux determination. All flux densities were determined from in-scan slices using the ADDSCAN. Upper limits are 3 times the rms noise. Except where noted in col. "Notes", all in-scan sources sizes are consistent with point sources. Jy n_S100 c indicates source confusion --- Star Visible stars? number=2 "Yes" denotes star(s) of magnitude 13 or brighter at photographic B or V within 45" in r.a. and 25" in decl. of the IRAS position. Star names are from either the SAO catalog or the Guide Star Catalog. Spectral classifications are given as recorded in the SIMBAD database. --- Notes Associations, notes number=3 (1) Also GSC 7421.0894 (2) Cirrus heated by nearby B8 IV star (Leene 1986). Deconvolved source sizes are W(12)=1.9", W(25)=3.0', W(60)=1.8', and W(100)=4.1". See Leene for integrated fluxes. (3) Mira variable (Feast, 1963) (4) A foreground eclipsing binary star (Tapia & Whelan, 1975). (5) Photometry for 2{mu}m sources associated with IRAS source is presented in table3. (6) Visible star in polarimetric study of Vrba, Strom & Strom 1976b (VSSb) or Vrba, Coyne & Tapia 1984 (VCT). (7) Deconvolved source sizes are W(12)=0.82', W(25)=1.1', and W(60)=1.0'. (8) IRAS LRS spectrum displays 10{mu}m emission feature plus "blue" continuum characteristics of an AGB star (Olnon & Raimond 1986) (9) Also GSC 7917.0901 which appears to be variable. (10) A foreground star which is double (Penny 1979). (11) A foreground star, HR 7232 (12) A foreground star, HR 7254 --- Near-infrared photometry of IRAS sources Name Source name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Vis Visibility number=1 "Yes" denotes either star was visible in focal plane camera (V <14 mag) or has published spectrum as referenced in col. "Notes". TT denotes a T Tauri star. --- l_Jmag limit flag on Jmag --- Jmag J magnitude number=2 Magnitudes at H and K are given in cols. Hmag and Kmag and are followed by their statistical one sigma errors in cols. e_Hmag and e_Kmag respectively, when they exceed absolute uncertainties. L photometry is quoted for a 4" (CTIO) or 6" aperture (IRTF). H and K photometry are quoted for a 6" apertures, except where noted in col. "Notes". mag l_Hmag limit flag on Hmag --- Hmag H magnitude number=2 Magnitudes at H and K are given in cols. Hmag and Kmag and are followed by their statistical one sigma errors in cols. e_Hmag and e_Kmag respectively, when they exceed absolute uncertainties. L photometry is quoted for a 4" (CTIO) or 6" aperture (IRTF). H and K photometry are quoted for a 6" apertures, except where noted in col. "Notes". mag e_Hmag rms uncertainty on Hmag mag l_Kmag limit flag on Kmag --- Kmag K magnitude number=2 Magnitudes at H and K are given in cols. Hmag and Kmag and are followed by their statistical one sigma errors in cols. e_Hmag and e_Kmag respectively, when they exceed absolute uncertainties. L photometry is quoted for a 4" (CTIO) or 6" aperture (IRTF). H and K photometry are quoted for a 6" apertures, except where noted in col. "Notes". mag e_Kmag rms uncertainty on Kmag mag l_Lmag limit flag on Lmag --- Lmag L magnitude number=2 Magnitudes at H and K are given in cols. Hmag and Kmag and are followed by their statistical one sigma errors in cols. e_Hmag and e_Kmag respectively, when they exceed absolute uncertainties. L photometry is quoted for a 4" (CTIO) or 6" aperture (IRTF). H and K photometry are quoted for a 6" apertures, except where noted in col. "Notes". mag u_Lmag Uncertainty flag on Lmag --- Obs Type of observations (CTIO or IRTF) --- Notes Notes number=3 Source names from Glass & Penston 1975 (GP), Vrba, Strom, & Strom 1976a (VSS), Vrba, Strom, & Strom 1976b (VSSb), Marraco & Rydgren 1981 (H{alpha}), Vrba, Coyne, & Tapia 1984 (VCT), and the Guide Star Catalog (GSC, Laskeret al.1990). d: Magnitude could be slightly underestimated due to faint source in sky annulus. e: Spectral type from Vrba & Rydgren 1984. f: Companion to HD 176386. Magnitudes could be slightly overestimated due to contamination from primary. g: Spectral type from Marraco & Rydgren 1981. --- Marie-Jose Wagner, Patricia Bauer CDS 1995 Mar 08 UNKNOWN UNKNOWN Keypunched at CDS J_ApJ_397_520.xml Dynamical properties of compact groups of galaxies. J/ApJ/399/353 J/ApJ/399/353 Radial velocities in Hickson compact groups Dynamical properties of compact groups of galaxies. P Hickson C Mendes de Oliveira J P Huchra G G C Palumbo Astrophys. J. 399 353 1992 1992ApJ...399..353H VII/85 : Catalogue of compact groups of galaxies (Hickson, 1982) J/A+AS/117/39 : Far-IR properties of Hickson Compact Groups (Allam+, 1996) J/ApJ/380/30 : LF of Compact Groups (Mendes de Oliveira+ 1991) Galaxies, optical Redshifts Velocity dispersion galaxies: clusters: general galaxies: distances and redshifts galaxies: ISM galaxies: luminosity function, mass function Radial velocities have been observed for 457 galaxies in the 100 Hickson compact groups (Hickson =1982ApJ...255..382H; catalog <VII/85>). Brighter galaxies were observed over the period 1984-1986, using the 1.5m telescope of the F.L. Whipple Observatory on Mt. Hopkins, Arizona, in wavelength range 470-710nm; the remaining fainter galaxies were observed with the Canada-France-Hawaii Telescope (CFHT). These velocities are listed in table2. Dynamical parameters were derived for 92 of the 100 groups, which are listed in table3; Hubble constant was assumed to be Ho=100km/s/Mpc.
Velocity data for galaxies HCG Hickson Group number <VII/85> --- m_HCG Galaxy in HCG group --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec RVhel Heliocentric velocity km/s e_RVhel Estimated rms in RVhel km/s q_RVhel Confidence code on RVhel the confidence code is 0 = highest confidence: spectral features clearly visible 1 = lower confidence: spectral features not clearly visible 2 = lowest confidence: very noisy spectra with no obvious features. Only 3 galaxies have q_RVhel=2. --- Group Dynamical Properties HCG Group number --- z Group Redshift derived from the median galaxy heliocentric velocity --- n Number of galaxies with accordant velocities --- log(sV) Radial velocity dispersion km/s log(V) Estimated instrinsic 3D velocity dispersion km/s log(R) Median projected separation kpc log(Ho.tc) Crossing time (expressed in 1/Ho units) --- log(Mv) Viral mass of group in log. scale g log(Mp) Projected mass g log(Ma) Average mass g log(Mm) Median mass g log(M) Adopted mass g log(L) Total blue luminosity of the accordant galaxies W log(M/L) Mass-to-light ratio Sun log(rho) Mass density g/cm3 Francois Ochsenbein CDS 1996 Aug 23 UNKNOWN UNKNOWN Prepared via OCR and proofread by Heinz Andernach in April 1995. J_ApJ_399_353.xml Microjansky source counts and spectral indices at 8.44 GHz J/ApJ/405/498 J/ApJ/405/498 Counts and spectral indices at 8.44GHz Microjansky source counts and spectral indices at 8.44 GHz R A Windhorst E B Fomalont R B Partridge J D Lowenthal Astrophys. J. 405 498 1993 1993ApJ...405..498W cosmic microwave background galaxies: evolution galaxies: starburst radio continuum: galaxies surveys We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18<~V<~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}<2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is <36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.
Catalog of 8.44 GHz Radio Sources in the Linx.2 Field Catalog of 8.44 GHz Radio Sources in the Cepheus Field Name Source name --- n_Name Source with an asterisk is not in the complete sample --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s e_RAs One sigma error on right ascension s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec e_DEs One sigma error on declination arcsec S8.44 Integrated sky flux density at 8.44GHz uJy e_S8.44 One sigma error on integrated sky flux density uJy l_SizeM When '<' the source is an unresolved source and it's given the 1.5{sigma} upper limit on the Gaussian major axis --- SizeM Deconvolved Gaussian source size (FWHM): major axis arcsec e_SizeM Error on major axis arcsec Sizem Deconvolved Gaussian source size (FWHM): minor axis arcsec e_Sizem Error on minor axis arcsec PA Position angle of major axis deg e_PA Error on position angle deg Weight Source weight in the 8.44 GHz counts --- S(p) Measured peak flux density on the 10arcsec resolution image uJy e_S(p) One sigma error on measured peak flux density uJy S(int) Resulting integrated flux density on the 10 arcsec image uJy e_S(int) One sigma error on resulting integrated flux density uJy James Marcout, Simona Mei CDS 1995 May 11 UNKNOWN UNKNOWN * March 1993: Number A075 in H. Andernach's list, transformed from original LaTeX provided by the author * Completed at CDS J_ApJ_405_498.xml Far-infrared emission from the intracluster medium. J/ApJ/405/94 J/ApJ/405/94 Far-infrared emission from 5 galaxy clusters Far-infrared emission from the intracluster medium. M W Wise R W O'Connell J N Bregman M S Roberts Astrophys. J. 405 94 1993 1993ApJ...405...94W II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989) Clusters, galaxy Infrared sources Spectra, infrared galaxies: clusters: general infrared: galaxies intergalactic medium We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.
Extracted point sources Cluster Cluster name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec PSC Point Source designation, generally not in IRAS-PSC (Cat. <II/125>) --- F60umExt Extracted point source 60um flux Jy F60umPSC IRAS-PSC or FSS (Cat. <II/156>) 60um flux Jy F100umExt Extracted point source 100um flux Jy F100umPSC IRAS-PSC or FSS 100um flux Jy r/rA Radius in Abell radius --- James Marcout, Patricia Bauer CDS 1998 Feb 26 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_405_94.xml A Catalog of Stellar Lyman-Alpha Fluxes J/ApJ/408/305 J/ApJ/408/305 Cat of Stellar Lyman-Alpha Fluxes A Catalog of Stellar Lyman-Alpha Fluxes W B Landsman T Simon ApJ 408 305 1993 1993ApJ...408..305L Photometry, hydrogen-line Stars, emission The data file gives the measured Lyman alpha flux or upper limits for 275 stars as derived from IUE spectra. The file is a subset of Table 1 of Landsman and Simon in that when a star had multiple measurements, only the best measurement is included in this table. The spectral types, V and B-V magnitudes in the table are culled from various sources as described in the paper. Most of the measurements are derived from low-dispersion spectra, and those derived from high- dispersion spectra are flagged. Each measurement was assigned a data quality code according to the signal to noise after removal of the diffuse Lyman alpha background emission. -1 - upper limit 1 - good quality 2 - fair quality 3 - poor quality 4 - contains saturated pixels The final column gives the ratio of the Ly alpha flux to the total bolometric flux of the star, determined as described in the paper. A roundoff was applied to the fluxes listed here to give the fluxes listed in Table 1 of Landsman and Simon.
Lyman-alpha fluxes Name Star Name --- HD HD number (0 if none) --- SpT Spectral Type --- V V magnitude mag B_V B-V color mag Image IUE SWP image number --- ExpTim IUE Exposure Time sec Disp 'H' if high-dispersion spectrum --- UpLim '<' if Ly flux is an upper limit --- LyFlux Ly alpha flux (in 10-14 erg cm-2 s-1 A-1) 10-13W/m2/nm Qual Measurement quality Each measurement was assigned a data quality code according to the signal to noise after removal of the diffuse Lyman alpha background emission. -1 - upper limit 1 - good quality 2 - fair quality 3 - poor quality 4 - contains saturated pixels -------------------------------------------------------------------------------- Remarks and Modifications: The file has been checked by the CDS procedure anafile for compliance with the format table. --- UpLim '<' if Ly flux is an upper limit --- LyNorm Normalized Flux [in 10-7 x normalization] 10-7 N. Paul M. Kuin NASA/NSSDC/ADC 1994 Jul 18 J_ApJ_408_305.xml Far-ultraviolet stellar photometry: a field in Monoceros J/ApJ/408/484 J/ApJ/408/484 Far-UV photometry of a field in Monoceros Far-ultraviolet stellar photometry: a field in Monoceros E G Schmidt G R Carruthers Astrophys. J. 408 484 1993 1993ApJ...408..484S J/ApJS/89/259 : another observation in a field in Orion Photometry, ultraviolet FUV photometry of stars in a field in Monoceros in the wavelength range from 1230 to 1600 A has been carried out using data from an electrographic Schmidt camera carried on a sounding rocket. Ultraviolet magnitudes were extracted for 602 objects in the field. Fifty-eight percent were tentatively identified with visible stars using the SIMBAD data base while another 25 percent are blends of objects too close together to separate with the resolution used.
Objects detected in the UV No Number of the star --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin m1367 Far UV magnitude mag Name Identification (from SIMBAD) of the star --- mag V or P magnitude mag n_mag P if mag is photographic --- Sp Spectral type --- Francois Ochsenbein CDS 1993 Dec 23 Edward Schmidt (eschmidt@unlinfo.unl.edu) J_ApJ_408_484.xml The Hubble Space Telescope Snapshot Survey. IV A Summary of the Search for Gravitationally Lensed Quasars J/ApJ/409/28 J/ApJ/409/28 Gravitationally Lensed Quasars The Hubble Space Telescope Snapshot Survey. IV A Summary of the Search for Gravitationally Lensed Quasars D Maoz J N Bahcall D P Schneider N A Bahcall S Djorgovski A Gould S Kirhakos R Doxsey G Meylan B Yanny Astrophys. J. 409 28 1993 1993ApJ...409...28M Gravitational lensing QSOs The Snapshot Survey was a search for cases of gravitational lensing among intrinsically-luminous, high-redshift quasars using the Hubble Space Telescope (HST) Planetary Camera (PC). The accompanying ASCII tables summarize the results of the survey.
The Snapshot Survey was a search for cases of gravitational lensing among intrinsically-luminous, high-redshift quasars using the Hubble Space Telescope (HST) Planetary Camera (PC). Bahcall et al. (1992a; hereafter Paper I) described the objectives of the survey, its mode of operation, the sample definition, and the initial results of a small sample. Maoz et al. (1992b, 1993a, 1993b hereafter Papers II, III, and IV) reported results from a progressively larger sample and compared the observed lensing frequency to existing theoretical models. The discovery of a possible sub-arcsecond lens system, the z=3.8 quasar 1208+1011, reported by Maoz et al. (1992a) and Magain et al. (1992), was followed by HST multi-color imaging and spectroscopy as described in Bahcall et al. (1992b) and in Bahcall et al. (1992c), respectively. Star counts based on the Snapshot Survey images are described in Gould, Bahcall, and Maoz (1993). For all objects in the Survey, finding charts and astrometric positions appear in Schneider et al. (1992). The accompanying tables, published in Paper IV, summarize the results of the Snapshot Survey for gravitationally lensed quasars. Table_1a.dat combines the results from Papers II, III, and IV into one list ordered by R.A. These tables have more accurately measured quasar magnitudes, and minor corrections have been made in some of the entries listed in the tables in previous papers, so that the present list superseded previous data summaries. Table_1b.dat lists the Paper I observations in the same format as table_1a.dat. Some of the exposures are only 120s (program 3034) and about half of the initial exposures were through the F785LP filter (similar to I), rather than the F555W filter. We have included in table_1b.dat only quasars that were not subsequently re-observed. These files can be merged without repetition. Exposures through the F785LP filter are marked with an "I" in the V_obs column.
Summary of Full Program Observations Summary of Successful Pilot Observations name Quasar name, without prefixes (1950 coor.) blank indicates repeated observation of preceding quasar --- altna Veron name --- date Date Observed --- HST HST Program Number --- chip PC chip showing object --- XY Central coordinate of quasar The coordinate of the center of the mosaic (not the chip) is 1, 1 pix off Offset from designated position on chip 6 arcsec drift Drift rate (g = guided exposure) marcsec V_obs Observed V (I indicates F785LP filter) mag V_ver Magnitude tabulated by Veron mag disc Discovery method R = radio selected C = selected by color S = Emission lines in spectrum O = Other (e.g. variability) --- redsh Redshift km/sec M Absolute magnitude mag note Notes An See "Notes on Individual Objects" in Paper n of Snapshot series. B Guided exposure, but quasar offset by $12"$ for unknown reasons. C Quasar image split between PC-6 and PC-7. D Quasar not verified to be in the field of view, but likely present based on brightness and/or expected absence of additional objects (see paper IV). F Possibly some point-spread function asymetry at $0.1-0.2"$ scales. E Quasar just off PC-8. G Identification uncertain. H Quasar image split between PC-7 and PC-8. J Poor fine-lock guiding attempt; multiple/trailed images. K Quasar image split between PC-5 and PC-6. L Cosmic ray event on or near quasar image core. --- D. Maoz Inst. Adv. Studies N.G. Roman NSSDC/ADC 1994 Aug 04 J_ApJ_409_28.xml IRAS variables as galactic structure tracers: classification of the bright variables. J/ApJ/411/188 J/ApJ/411/188 IRAS variables as galactic structure tracers IRAS variables as galactic structure tracers: classification of the bright variables. L E Allen S G Kleinmann M D Wwinberg Astrophys. J. 411 188 1993 1993ApJ...411..188A Galaxy: structure infrared: stars stars: variables: other *** No Description Available ***
Merging of tables 1A (M giants), 1B (C or S stars), 1C (not M C S), and 1D (other) Class Classes (is taken from table) M = M giants (table 1A) C = Carbon or S stars (table 1B) c = sources neither C nor S (table 1C) d = sources could not be classified (table 1D) --- IRAS IRAS name --- Rem Remark, see below number=1 Remarks are a: associated with M17; classified K0 by Bidelman b: associated with an HII region c: associated with radio source PKS 1952+017 d: associated with a F7/8V star e: associated with CZ Aps, Mira of unknown period f: associated with V545 Oph, Mira (223 days) g: associated with TMSS-30436E h: associated with EF Sgr, Mira (375 days) i: associated with TMSS-30483E --- Sp Spectral type --- r_Sp Reference of Sp number=2 References of Spectral types [1] te Lintel Hekkert 1990 [2] Kholopov et al. 1985 [3] Bidelman 1980 or 1992 [4] Eder. Lewis & Terzian 1988 or Lewis, Eder & Terzian 1990 [5] Price & Murdoch 1983 [6] Kleinmann, Gillett & Joyce 1981 [7] Kukarkin et al. 1981 [8] Zuckerman & Dyck 1986 [9] SAO star catalogue 1966 [10] Stephenson 1989 [11] Kastner 1990 --- RadSp Radio Spectrum --- r_Sp Reference of RadSp number=2 References of Spectral types [1] te Lintel Hekkert 1990 [2] Kholopov et al. 1985 [3] Bidelman 1980 or 1992 [4] Eder. Lewis & Terzian 1988 or Lewis, Eder & Terzian 1990 [5] Price & Murdoch 1983 [6] Kleinmann, Gillett & Joyce 1981 [7] Kukarkin et al. 1981 [8] Zuckerman & Dyck 1986 [9] SAO star catalogue 1966 [10] Stephenson 1989 [11] Kastner 1990 --- LRS IRAS Low Resolution Spectra classification --- IRC Two-micron sky survey designation --- GCVS General Catalogue of Variable Star designation --- VType Variable type (period in days) --- r_VType Reference of VType number=3 References of Variability type for M type [1] Herman & Habing 1985 [2] GCVS [3] Lockwood 1985 [4] Jones et al. 1990 [5] Engels 1982 --- F12 Flux at 12um Jy l_F25 Limit flag on F25 --- F25 Flux at 25um Jy l_F60 Limit flag on F60 --- F60 Flux at 60um Jy l_log.DF12 Limit flag on log.DF12 --- log.DF12 Flux density variation from IRAS Working Survey Data Base at 12um Jy l_log.DF25 Limit flag on log.DF25 --- log.DF25 Flux density variation from IRAS Working Survey Data Base at 25um Jy l_log.DF60 Limit flag on log.DF60 --- log.DF60 Flux density variation from IRAS Working Survey Data Base at 60um Jy u_log.DF60 Uncertainty flag (:) on log.DF60 --- James Marcout, Francois Ochsenbein CDS 1994 Mar 18 UNKNOWN UNKNOWN Keypunched at CDS; remarks and references have been renumbered at CDS J_ApJ_411_188.xml Multiwavelength Monitoring of the BL Lac Object PKS 2155-304 I. The IUE Campaign J/ApJ/411/614 J/ApJ/411/614 Monitoring of PKS 2155-304 I. The IUE Campaign Multiwavelength Monitoring of the BL Lac Object PKS 2155-304 I. The IUE Campaign C M Urry L Maraschi R Edelson A Koratkar J Krolik G Madejski E Pian G Pike G Reichert A Treves W Wamsteker R C Bohlin J N Bregman W Brinkmann L Chiappetti T Courvoisier A V Filippenko H Fink I M George Y Kondo P G Martin H R Miller P O'Brien J M Shull M Sitko A E Szymkowiak G Tagliaferri S Wagner R Warwick Astrophys. J. 411 614 1993 1993ApJ...411..614U BL Lac objects Spectra, ultraviolet Daily monitoring of PKS 2155-304 with the IUE satellite throughout November 1991 revealed dramatic large-amplitude rapid variations in the UV flux of this BL Lac object. Many smaller, rapid flares are superposed on a general doubling of the intensity. During the five-day period when sampling was roughly continuous, the rapid flaring had an apparent quasi-periodic nature, with peaks repeating every 0.7 day. The short- and long-wavelength UV light curves are well correlated with each other, and with the optical light curve deduced from the Fine Error Sensor on IUE. The formal lag is zero, but the cross-correlation is asymmetric in the sense that the shorter wavelengthemission leads the longer. The UV spectral shape varies a small but significant amount. The correlation between spectral shape and intensity is complex. The sign of the correlation is consistent with the nonthermal acceleration processes expected in relativistic plasmas, so that the present results are consistent with relativistic jet models, which can also account for quasi-periodic flaring.
Log of IUE observations num IUE image number --- time Start time (day of November 91) in UT d exp Exposure time min Vmag V Magnitude (from FES counts) mag obsrvtry IUE Observatory (G=Goddard or V=Vilspa) --- Power-law fits to IUE spectra num IUE image number SWP images first, then LWP --- time Observation midpoint (day of November 91) U d flux Flux at 1400/2800 angstrom flux at 1400 A for SWP and at 2800 A for LWP 10+15mW/m2/nm e_flux Error on flux 10+15mW/m2/nm alpha Spectral index --- e_alpha Error on spectral index --- chisq Chi squared of spectral fit --- Power-law fits to merged IUE spectra SWP_num Image numbers SWP --- LWP_num Image numbers LWP --- time Observation midpoint (day of November) d flux Flux at 2000 angstrom 10+15mW/m2/nm e_flux Error on flux at 2000 angstrom 10+15mW/m2/nm alpha Spectral index --- e_alpha Error on spectral index --- chisq Chi squared of spectral fit --- J. Pesce STScI 1995 Mar 21 This work was supported in part by NASA grant NAG 5-1034. If there are comments/corrections/questions, please contact: C. Megan Urry cmu@stsci.edu STScI Tel.: 410-338-4593 3700 San Martin Drive FAX: 410-338-4767 Baltimore, MD 21218 J_ApJ_411_614.xml The RR Lyrae variables in the globular cluster M68 J/ApJ/412/183 J/ApJ/412/183 RR Lyr in M68 The RR Lyrae variables in the globular cluster M68 C M Clement S Ferance N R Simon Astrophys. J. 412 183 1993 1993ApJ...412..183C globular clusters: individual (M 68) RR Lyrae variable stars: oscillations *** No Description Available ***
*B magnitudes for 30 RR Lyrae variables in M68 HJD Heliocentric Julian Date d V1 B magnitude of star V1 mag V2 B magnitude of star V2 mag V3 B magnitude of star V3 mag V4 B magnitude of star V4 mag V5 B magnitude of star V5 mag V6 B magnitude of star V6 mag V7 B magnitude of star V7 mag V8 B magnitude of star V8 mag V9 B magnitude of star V9 mag V11 B magnitude of star V11 mag V13 B magnitude of star V13 mag V14 B magnitude of star V14 mag V15 B magnitude of star V15 mag V16 B magnitude of star V16 mag V18 B magnitude of star V18 mag V19 B magnitude of star V19 mag V20 B magnitude of star V20 mag V21 B magnitude of star V21 mag V22 B magnitude of star V22 mag V23 B magnitude of star V23 mag V24 B magnitude of star V24 mag V25 B magnitude of star V25 mag V26 B magnitude of star V26 mag V28 B magnitude of star V28 mag V29 B magnitude of star V29 mag V30 B magnitude of star V30 mag V31 B magnitude of star V31 mag V32 B magnitude of star V32 mag V33 B magnitude of star V33 mag V34 B magnitude of star V34 mag *Elements of the RR Lyrae variables in M68 (based on the Las Campanas observations) Name Star name --- Type Bailey type --- X X position relative to the cluster center according to Sawyer Hogg (1973) arcsec Y Y position relative to the cluster center arcsec Period Primary period d Bmag Mean B magnitude mag A(B) B amplitude mag Patricia Bauer CDS 1994 Sep 19 AAS CD-ROM Series, Volume 1, 1993 J_ApJ_412_183.xml On the redshift-apparent size diagram of double radio sources J/ApJ/413/453 J/ApJ/413/453 On the redshift-apparent size diagram of double On the redshift-apparent size diagram of double radio sources K Nilsson M J Valtonen J Kotilainen T Jaakkola Astrophys. J. 413 453 1993 1993ApJ...413..453N cosmology: observations quasars: general radio continuum: galaxies *** No Description Available ***
Double radio source data IAU IAU name --- Name Other name --- z Spectroscopically measured redshift --- LAS Largest angular size arcsec size True linear size kpc logL Radio luminosity in the frequency interval 10 MHz-10 GHz (erg/s) 10-7W alpha Spectral index at the high-frequency end of the spectral range --- Id Type of the central object: G: galaxy Q: quasar --- ref References (in file reftab1) --- References to table1 ref Reference number --- Names Authors' names --- Patricia Bauer CDS 1994 Jul 07 Kari Nilsson <kani@sirius.astro.utu.fi> J_ApJ_413_453.xml 30 Doradus: ultraviolet and optical stellar photometry J/ApJ/413/604 J/ApJ/413/604 30 Dor 30 Doradus: ultraviolet and optical stellar photometry J K Hill R C Bohlin K -P Cheng M N Fanelli P Hintzen R W O'Connell M S Roberts A M Smith E P Smith T P Stecher Astrophys. J. 413 604 1993 1993ApJ...413..604H dust, extinction ISM: individual (30 Dor) Magellanic Clouds techniques: photometric ultraviolet: stars Ultraviolet Imaging Telescope (UIT) UV magnitudes in four bands, together with optical B magnitudes, are presented for up to 314 early-type stars located in a 9.7 x 9.7 arcmin field centered on R136. The magnitudes have an rms uncertainty estimated at 0.10 mag from a comparison between the UIT magnitudes and the IUE spectra. Spectral types and E(B-V) color excesses are estimated. The mean color excesses following the two extinction curves agree well with the predictions of the two-component extinction model of Fitzpatrick and Savage (1984). However, the degree of nebular extinction is found to vary systematically by large amounts over the 30 Dor field. The minimum of nebular extinction in the central parts of the nebula suggests that dust has been expelled from this region by stellar winds. It is suggested that the form of the UV extinction curve can be understood as a consequence of the evolutionary state of the stellar population responsible for making the dust grains.
Stellar UV and B photometry UIT Ultraviolet Imaging Telescope (UIT) number --- dRA Right ascension (2000) offset from R136 (= 5:38:42) arcsec dDE Declination (2000) offset from R136 (= -69:6:1) arcsec m162 m_162 magnitude in the UIT B5 band mag m189 m_189 magnitude in the UIT A2 band mag m221 m_221 magnitude in the UIT A4 band mag m256 m_256 magnitude in the UIT A5 band mag B B magnitude in the optical B band mag Fit spectral types and extinctions UIT Ultraviolet Imaging Telescope (UIT) number --- SP Estimated spectral type --- E(B-V)F Estimated F curve E(B-V)_F (Fitzpatrick 1985) mag E(B-V)FS Estimated FS curve E(B-V)_FS (Fitzpatrick 1984) mag RMS Estimated rms magnitude differences between the best-fit model and the observations --- table3.tex LaTeX version of table3 table5.tex LaTeX version of table5 environ.tex Format for LaTeX version Patricia Bauer CDS 1994 Sep 16 AAS CD-ROM series, Volume 1, 1993 J_ApJ_413_604.xml The faintest stars: the luminosity and mass functions at the bottom of the main sequence. J/ApJ/414/279 J/ApJ/414/279 Faintest stars The faintest stars: the luminosity and mass functions at the bottom of the main sequence. C G Tinney Astrophys. J. 414 279 1993 1993ApJ...414..279T stars: formation stars: low-mass, brown dwarfs stars: luminosity function, mass function techniques: photometric We present infrared K-band photometry of complete samples of VLM candidates constructed from IIIaF and IVN plates in 10 fields taken as part of the POSSII and UKSRC surveys. Using the I-K colors constructed for these stars we estimate a bolometric luminosity function which extends to MBol=13.75. We find significant evidence for a luminosity function decreasing toward these luminosities.
Areas and limits surveyed NField Field identification letter --- Name Field designation --- RAh Field right ascension 1950 h RAm Field right ascension 1950 min DEd Field declination 1950 deg Master Master plate --- n_Master Note on Master number=1 Objects were selected from the areas of I11499 which does not overlap with N3601 (the plate used to select the Fld 832-1 sample) --- Slaves Slave plates --- Area Area in which IIIaF and IVN plates are coincident deg+2 Imin Lower limit of I magnitude interval mag Imax Upper limit of I magnitude interval mag R-Imax Upper limit of R-I color mag Limits A 'y' means that the sample includes upper limits, constructed from pairs IVN plates and IIIaF non-detections --- Survey samples in each POSSII/UKSRC field selected by photographic color Miscellaneous interesting objects (I-K>3.0) not part of survey sample NField Field designation as in table1 --- Name Object name --- n_Name Note on Name number=1 d: the following pairs of objects lie in the overlap regions between two plates and were assigned duplicate names; - in table2: 213-16596 = 263-68812; 213-19088 = 263-72846; 831-161058 = 832-3494; 831-165166 = 832-7464; 890-4633 = 891-137643. - in table3: 263-78128 = 262-3688 b: in table3, 513-42404 was discovered as an infrared companion to the star TVLM 513-4240 --- RAh Right ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Iphot I magnitude from photographic observations on the Palomar 60" telescope mag (R-I)Phot (R-I) color from photographic observations on the Palomar 60" telescope mag q_(R-I)Phot A 'l' indicates upper limit object, object detected above (IPhot)lim, but not detected on a IIIaF plate --- Iccd I magnitude from CCD camera on the Palomar 60" telescope mag (R-I)ccd (R-I) color from CCD camera on the Palomar 60" telescope mag Kcam K magnitude measured at Las Campanas mag q_Kcam Note on Kcam number=2 a: Photometry good to +/-0.05mag b: Photometry good to +/-0.10mag c: Photometry only good to +/- 0.25mag ':': Object barely detected and the photometry is only good to +/-0.5mag e: Preliminary photometry from an IRTF run on 1992 October 23-26 n: not detected --- Kpal K magnitude measured at Palomar mag q_Kpal Note on Kpal number=2 a: Photometry good to +/-0.05mag b: Photometry good to +/-0.10mag c: Photometry only good to +/- 0.25mag ':': Object barely detected and the photometry is only good to +/-0.5mag e: Preliminary photometry from an IRTF run on 1992 October 23-26 n: not detected --- Kirtf K magnitude measured at Nasa Infrared Telescope Facility (IRTF) mag q_Kirtf Note on Kirtf number=2 a: Photometry good to +/-0.05mag b: Photometry good to +/-0.10mag c: Photometry only good to +/- 0.25mag ':': Object barely detected and the photometry is only good to +/-0.5mag e: Preliminary photometry from an IRTF run on 1992 October 23-26 n: not detected --- Kmn Mean K magnitude mag q_Kmn Note on Kmn number=2 a: Photometry good to +/-0.05mag b: Photometry good to +/-0.10mag c: Photometry only good to +/- 0.25mag ':': Object barely detected and the photometry is only good to +/-0.5mag e: Preliminary photometry from an IRTF run on 1992 October 23-26 n: not detected --- I-K I-K color (calculated using ICDD when available, and otherwise using IPhot) mag q_I-K When 'c', this object shows possible evidence of variability --- Marie-Jose Wagner, Patricia Bauer CDS 1994 Oct 24 UNKNOWN UNKNOWN keypunched at CDS J_ApJ_414_279.xml Thomas-Fermi calculations of atoms and matter in magnetic neutron stars: effects of higher Landau bands J/ApJ/416/276 J/ApJ/416/276 Eq. of State in Magnetic Neutron Stars Thomas-Fermi calculations of atoms and matter in magnetic neutron stars: effects of higher Landau bands O E Rognvaldsson I Fushiki E H Gudmundsson C J Pethick J Yngvason Astrophys. J. 416 276 1993 1993ApJ...416..276R Atomic physics Models, evolutionary Stars, variable Landau levels stars: neutron Thomas-Fermi approximation This catalog is based on the calculated equation of state in cold dense matter. Each table in the catalog lists bulk properties of Fe-56 in a magnetic field ranging from one million to 1000 million Tesla.
We calculate the equation of state for cold dense matter in high magnetic fields in the Thomas-Fermi approximation, taking all Landau levels into account. Total energies and chemical potentials for atoms and matter are also calculated, and we present detailed profiles of the electron density as a function of the distance from the atomic nucleus for various values of the magnetic field strength and total matter density. The profiles show a Landau shell structure, which for iron atoms at low pressure is particularly pronounced for magnetic fields of order 10^11^ G. In compressed matter this structure is reflected in a high compressibility when the density is such that electrons at the boundary of a unit shell start to occupy a new Landau band. This leads to an oscillatory behavior of the density gradient as a function of depth in the surface layers of magnetic neutron stars.
1 million (10^6^) Tesla 3 million (10^6.5^) Tesla 10 million (10^7^) Tesla 30 million (10^7.5^) Tesla 100 million (10^8^) Tesla 300 million (10^8.5^) Tesla 1000 million (10^9^) Tesla density density of matter kg/m3 radius radius of cell m pressure pressure Pa eatom total energy of atom (in 1.602E-16J) keV chempot chemical potential (in 1.602E-16J) keV zg12 depth.(surface gravity)/(10^12 m/s^2) m N. Paul Kuin ADC 1996 Jul 09 J_ApJ_416_276.xml The Dynamics of the Galaxy Cluster Abell 2634 J/ApJ/416/36 J/ApJ/416/36 Dynamics of the Galaxy Cluster Abell 2634 The Dynamics of the Galaxy Cluster Abell 2634 J Pinkney G Rhee J O Burns J M Hill W Oegerle D Batuski P Hintzen Astrophys. J. 416 36 1993 1993ApJ...416...36P Clusters, galaxy Redshifts All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L. Velocities are presented for 254 galaxies in the rich Abell cluster 2634. Positions are given for 274 additional galaxies for which further investigation is desirable.
The observations ID Galaxy ID --- RAh Right Ascension (2000) h RAm Right Ascension (2000) min RAs Right Ascension (2000) s DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec cz1 Velocities from high correlation peaks km/s cz2 Velocities from low correlation peaks km/s e_cz1 Uncertainty estimated from correlation km/s Other objects ID Galaxy ID --- RAh Right Ascension (2000) h RAm Right Ascension (2000) min RAs Right Ascension (2000) s DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec N. G. Roman NASA/NSSDC/ADC 1994 Jul 18 J_ApJ_416_36.xml The Mount Wilson Observatory Metallicity index, Crv: comparison with other photometric systems J/ApJ/416/787 J/ApJ/416/787 The Mount Wilson Observatory Metallicity index, Crv: The Mount Wilson Observatory Metallicity index, Crv: comparison with other photometric systems W H Soon Q Zhang S L Baliunas R L Kurucz Astrophys. J. 416 787 1993 1993ApJ...416..787S stars: abundances stars: late-type techniques: spectroscopic *** No Description Available ***
Data for dwarfs Data for giants HD HD designation --- m_HD Multiplicity index on HD designation --- n_HD Note for HD 36389 number=1 Note that the reddest giant on the list HD 36389 had b-y = 1.440 and is not plotted in all the (b-y)-dependent plots. --- Name Other name --- <Crv> Time averaged spectrophotometric index Crv = 2.5 log (N_R/N_V) number=2 N_R and N_V are the counts in the two wider windows (20A) labeled as R_4001 and V_3901, centered at 4001 and 3901 A respectively. mag o_<Crv> Number of observed points --- e_<Crv> Standard deviation of observed points --- b-y Observed b-y index mag m1 Observed m1 index mag c1 Observed c1 index mag V-K Observed V-K index mag THETAeff Observed stellar effective temperature (THETAeff= 5040/Teff, Teff in K) --- log(g) Observed surface gravity cm/s2 [Fe/H]1 Scaled iron abundance --- n_[Fe/H] ',' indicates a metallicity interval --- [Fe/H]2 Highest value of metallicity when n_[Fe/H] = , --- Dm magnitude difference of the two components for double stars mag Sep Maximum observed separation for double stars arcsec Period Orbital period for double stars The symbols SBa and SB identify the primary star associated with a known or suspected spectroscopic binary system. --- Patricia Bauer CDS 1994 Jul 11 Willie Soon <wsoon@cfassp34.harvard.edu> J_ApJ_416_787.xml Proper motions and radial velocities in the globular cluster M22 and the cluster distance J/ApJ/420/612 J/ApJ/420/612 Proper motions & radial velocities in M22 Proper motions and radial velocities in the globular cluster M22 and the cluster distance R C Peterson K M Cudworth Astrophys. J. 420 612 1994 1994ApJ...420..612P Clusters, globular Radial velocities Stars, distances astrometry globular clusters: individual (M 22) stars: distances techniques: radial velocities The distance to the globular cluster M22 is reexamined from new radial-velocity data and revised proper motions. Proper motions are rederived for 672 stars in the field of M22 using plate constant solutions from which stars of large proper motions have been removed, to reduce systematic errors which depend on coordinates. Radial velocities good to 1km/s have been obtained for 130 members of the globular cluster M22. The mean radial velocity is -148.8+/-0.8km/s. The radial velocity dispersion is 6.6+/-0.8km/s in the mean, and shows little if any dependence on distance from the cluster center over a 3'-7' annulus. Ignoring the small effect of rotation, a mass-to-light ratio M/L_V=0.85+/-0.15 in solar units is derived. The lack of stars moving faster than the escape velocity suggests strongly that a value M/L_V~1 applies to the cluster as a whole. This value is among the lowest observed for any globular cluster. Rotation is evident in both proper motions and radial velocities, and its position angle is in reasonable agreement with the major axis of the cluster's elongation. Its amplitude diminishes with radius, from ~6km/s for 1'<=r<= 3', to ~3km/s for 3'<=r<=7'. Rotation must be carefully modeled to determine an accurate distance to the cluster. From the simple approximation that the velocity dispersion is unaffected in the directions perpendicular to the streaming motion, a comparison of the dispersions in proper motion with those in radial velocity leads to a preliminary estimate for the distance of 2.6+/-0.3kpc, and a horizontal-branch magnitude M_V=0.71+/-0.27, using the reddening value E(B-V)=0.42 from M22 BHB stars.
Velocities for M22 members *Velocities for M22 field stars HJD-2440000 Julian date (-2440000) of each observation Julian date of each observation, or that of the first observation if the star was observed twice or more. d RAh Right ascension (equinox 1950.0) h RAm Right ascension (equinox 1950.0) min RAs Right ascension (equinox 1950.0) s DE- Declination sign --- DEd Declination (equinox 1950.0) deg DEm Declination (equinox 1950.0) arcmin DEs Declination (equinox 1950.0) arcsec Dist Radial distance from cluster center Radius and position angle from the center of the cluster, RA = 18h 33m 21.5s, DE = -23d 56m 44s, as measured by Shawl & White (1986AJ.....91..312S) arcmin PA Position angle positive north through east deg RV Measured radial velocity For all multiply observed stars, this is the weighted mean of the set of observations in Table 4. km/s e_RV Internal one-sigma uncertainty in RV The uncertainty is derived from the ratio R of the height of the cross-correlation peak relative to a typical noise fluctuation, according to the Tonry & Davis (1979AJ.....84.1511T) formula sigma_R=K/(1+R) (in km/s), with K=8.3 for sharp-lined spectra obtained with the Mount Hopkins echelle spectrographs. km/s Vmag V magnitude mag Memb Percent probability of membership % ID Identification First, when available, is the identification of Arp & Melbourne (1959AJ.....64...28A) or its extension by Lloyd-Evans (1975MNRAS.171..647L), with Roman numerals I-IV for the quadrants and V for the center. This is followed by identification from Alcaino (1977A&AS...29..383A) and the extension by Alcaino & Liller (1983AJ.....88.1330A), for which the annulus number precedes the number of the star. Last comes the variable number from Sawyer-Hogg (1973PDDO....3....6S), prefix V, no hyphen. If no other name is available, table2 list the Cudworth (1986AJ.....92..348C) number, preceded by C. --- Stars with multiple velocity measurements HJD-2440000 Julian date (-2440000) of each observation d RV Measured radial velocity km/s e_RV Internal uncertainty in RV km/s Vmag V magnitude mag ID Identification Arp & Melbourne (1959AJ.....64...28A) or its extension by Lloyd-Evans (1975MNRAS.171..647L), with Roman numerals I-IV for the quadrants. Sawyer-Hogg (1973PDDO....3....6S), prefix V, no hyphen. --- CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 06-May-1995 J_ApJ_420_612.xml The influence of bars on the chemical composition of spiral galaxies J/ApJ/424/599 J/ApJ/424/599 Abundances in barred spiral galaxies The influence of bars on the chemical composition of spiral galaxies P Martin J -R Roy Astrophys. J. 424 599 1994 1994ApJ...424..599M VII/112 : RC2 Catalogue (de Vaucouleurs+ 1976) Abundances H II regions galaxies: abundances galaxies: kinematics and dynamics galaxies: spiral galaxies: structure HII regions Imaging spectrophotometry in the nebular lines H{alpha}, H{beta}, [OIII]{lambda}5007 and [NII]{lambda}6584, using narrow-band interference filters, has been performed of 82, 55, and 79 H II regions in the barred spiral galaxies NGC 925, NGC 1073, and NGC 4303, respectively. The O/H abundance gradients were derived from the abundance indicators [O III]/H{beta} and [N II]/[O III], calibrated by Edmunds & Pagel (1984MNRAS.211..507E). The global O/H gradients in NGC 925 [{DELTA}log(O/H)/{DELTA}R=0.033dex/kpc] and NGC 1073 [{DELTA}log(O/H)/{DELTA}R=0.048dex/kpc] are flatter than the gradients observed in normal galaxies of the same morphological type. The abundance gradient in NGC 4303 is identical to that found in normal spiral galaxies. A comparison is made between the O/H gradients of normal galaxies and of a sample of galaxies showing a barred morphology it is concluded that the global abundance gradients of spiral galaxies with a barred structure are in general shallower than gradients of normal galaxies. The slopes of O/H gradients are analyzed as a function of two properties of bars: the relative length of the bar with respect to the size of the disk, and the bar ellipticity, defined by the axis ratio of the bar. It is found that gradients are flatter when the length or the ellipticity of the bar increases. This result is consistent with recent models of radial flows. These observations indicate that large-scale mixing of the interstellar gas occurs across the disks of barred spiral galaxies and affects the radial distribution of elements.
NGC 925 02 27.3 +33 35 NGC 1073 02 43.7 +01 23 NGC 4303 12 21.9 +04 28
Properties of H II regions in NGC 925 Properties of H II regions in NGC 1073 Seq Region sequential number --- log([OIII]/Hb) Corrected [O III]/H{beta} line ratio --- e_log([OIII]/Hb) rms uncertainty on log([OIII]/Hb) --- log([NII]/[OIII]) Corrected [N II]/[O III] line ratio --- e_log([NII]/[OIII]) rms uncertainty on log([NII]/[OIII]) --- log([NII/Ha) Corrected [N II/H{alpha} line ratio --- e_log([NII/Ha) rms uncertainty on log([NII/Ha) --- R/Reff Galactocentric distance corrected for inclination --- c(Hb) Logarithmic extinction at H{beta} --- e_c(Hb) rms uncertainty on c(Hb) --- O/H O/H gradient --- Properties of galaxies with abundance gradients with samples >=10 H II regions NGC Galaxy name --- Type Morphological type --- T T parameter (de Vaucouleurs et al., 1976, Cat. <VII/112>) --- i Inclination angle deg PA Position angle deg Dist Distance Mpc N Number of H II regions used to derive the O/H gradient --- Rad25 Radius at the 25 magnitude/arcsec^2^ isophote in blue light arcsec a Semi-major axis arcsec b Semi-minor axis arcsec Ebar Bar ellipticity (Ebar=10(1-b/a)) --- a/Rad25 a/Rad25 ratio --- Slope Slope of the global O/H gradient normalized for the adopted distance kpc-1 r_PA References for inclination & position angle number=1 References : 1: Vila-Costas & Edmunds 1992MNRAS.259..121V 2: Belley & Roy 1992ApJS...78...61B 3: Wevers et al. 1986A&AS...66..505W 4: Our study 5: England, Gottesman, & Hunter 1990ApJ...348..456E 6: Roy et al. 1996ApJ...460..284R 7: Walsh & Roy 1989ApJ...341..722W 8: Martin 1992, Ph.D. thesis, Univ. d'Aix-Marseille I 9: Oey & Kennicutt 1993ApJ...411..137O 10: Martin et al. 1989ApJ...345..707M 11: Warmels 1988A&AS...72...57W 12: Martin & Roy 1992ApJ...397..463M 13: Scowen, Dufour & Hester 1992AJ....104...92S 14: Zaritsky et al. 1994ApJ...420...87Z --- r_N References for N and slopes of gradients number=1 References : 1: Vila-Costas & Edmunds 1992MNRAS.259..121V 2: Belley & Roy 1992ApJS...78...61B 3: Wevers et al. 1986A&AS...66..505W 4: Our study 5: England, Gottesman, & Hunter 1990ApJ...348..456E 6: Roy et al. 1996ApJ...460..284R 7: Walsh & Roy 1989ApJ...341..722W 8: Martin 1992, Ph.D. thesis, Univ. d'Aix-Marseille I 9: Oey & Kennicutt 1993ApJ...411..137O 10: Martin et al. 1989ApJ...345..707M 11: Warmels 1988A&AS...72...57W 12: Martin & Roy 1992ApJ...397..463M 13: Scowen, Dufour & Hester 1992AJ....104...92S 14: Zaritsky et al. 1994ApJ...420...87Z --- James Marcout, Patricia Bauer CDS 1997 Mar 21 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_424_599.xml Initial mass functions from ultraviolet stellar photometry: a comparison of Lucke and Hodge OB Associations near 30 Doradus with the nearby field J/ApJ/425/122 J/ApJ/425/122 IMF from UV stellar photometry Initial mass functions from ultraviolet stellar photometry: a comparison of Lucke and Hodge OB Associations near 30 Doradus with the nearby field J K Hill J E Isensee R H Cornett R C Bohlin R W O'Connell M S Roberts A M Smith T P Stecher Astrophys. J. 425 122 1994 1994ApJ...425..122H Magellanic Clouds open clusters and associations: individual (30 Dor) stars: luminosity function, mass function ultraviolet: stars UV stellar photometry is presented for 1563 stars within a 40' circular field in the LMC, excluding the 10'x10' field centered on R136 investigated earlier by Hill et al. (1993). Magnitudes are computed from images obtained by the Ultraviolet Imaging Telescope in bands centered at 1615A and 2558A. Stellar masses and extinctions are estimated for the stars in associations using the evolutionary models of Schaerer et al. (1993), assuming the age is 4Myr and that the local LMC extinction follows the Fitzpatrick (1985) 30 Dor extinction curve. The estimated slope of the initial mass function (IMF) for massive stars (>15M_{sun}_) within the Lucke and Hodge (LH) associations is {gamma}=-1.08+/-0.2. Initial masses and extinctions for stars not within LH associations are estimated assuming that the stellar age is either 4Myr or half the stellar lifetime, whichever is larger. The estimated slope of the IMF for massive stars not within LH associations is {gamma}=-1.74+/-0.3 (assuming continuous star formation), compared with {gamma}=-1.35, and {gamma}=-1.7+/-0.5, obtained for the Galaxy by Salpeter (1955) and Scalo (1986), respectively, and {gamma}=-1.6 obtained for massive stars in the Galaxy by Garmany, Conti, & Chiosi (1982). The shallower slope of the association IMF suggests that not only is the star formation rate higher in associations, but that the local conditions favor the formation of higher mass stars there. We make no corrections for binaries or incompleteness.
Observed and fitted stellar data Star Running number of star --- X X offset from J2000 fiducial position RA=5h 38m 44s, Decl.=-69deg 6' 32" arcsec Y Y offset from J2000 fiducial position RA=5h 38m 44s, Decl.=-69deg 6' 32" arcsec m162 B5 band magnitude (1615 A) mag m256 A5 band magnitude (2558 A) mag LH Lucke and Hodge association number, or zero --- Mass Fitted mass solMass E(B-V) Fitted E(B-V) within 30 Dor mag rms rms magnitude difference between the observations and the best-fit model mag table2.tex LaTeX table version of table2.dat environ.tex LaTeX environment for table2.tex Lee Brotzman ADS 1994, Patricia Bauer [CDS] 25-Oct-1994 May 09 AAS CD-ROM series, Volume 2, 1994 J_ApJ_425_122.xml Orientation modeling of radio galaxy and quasar properties: evidence for a unified model. J/ApJ/427/125 J/ApJ/427/125 QSOs orientation modeling Orientation modeling of radio galaxy and quasar properties: evidence for a unified model. M L Lister J B Hutchings A C Gower Astrophys. J. 427 125 1994 1994ApJ...427..125L Galaxies, radio QSOs galaxies: active methods: statistical quasars: general radio continuum: galaxies We discuss the statistics of projection on the sky of a simple model for radio sources. The model has a core and two hot spots at unequal distance with an overall structure which is bent at the core. We examine the distributions or the observed sizes and bend angles in 114 quasars and 78 radio galaxies with z<2, from our own data. We find that the observations are well matched by this model with (a) a size distribution matching the observed one, (b) core-hotspot length differences between 0 and 45kpc, and (c) bend angles distributed between 0deg and ~25deg, where quasars are seen within 50deg of the source axis, and radio galaxies are seen at greater angles. We discuss the implications of these fits to unified models and source evolution.
Radio quasar data Name Quasar name --- n_Name Note number=1 d: These sources were remeasured using improved maps. --- z Redshift --- Q Core-hot spot distance ratio (see Fig 1). --- LAS Largest apparent size (see Fig.1). arcsec Size Size (assuming H_0_=100km/s/Mpc and q_0_=0.5) kpc Bend Bend angle deg Ref Reference number=2 References: GH : Gower & Hutchings (1984AJ.....89.1658G) HPG: Hutchings, Price & Gower(1988ApJ...329..122H) LHG: Lister, Hutchings & Gower (1994ApJ...427..125L) NH : Neff & Hutchings (1990AJ....100.1441N) NHG: Neff, Hutchings & Gower (1989AJ.....97.1291N) ---- D statistics for equal lobe (Q_intrinsic_=1) models D statistics for equal lobe (Q_intrinsic_.diff.1) models Bend1 Bend range (lower value) deg Bend2 Bend range (upper value) deg Db90 Goodness of fit statistic for size-bend distributions at phi=90 --- Dq90 Goodness of fit statistic for size-Q distributions at phi=90 --- D90 Total goodness of fit statistic at phi=90 --- Db60 Goodness of fit statistic for size-bend distributions at phi=60 --- Dq60 Goodness of fit statistic for size-Q distributions at phi=60 --- D60 Total goodness of fit statistic at phi=60 --- Db50 Goodness of fit statistic for size-bend distributions at phi=50 --- Dq50 Goodness of fit statistic for size-Q distributions at phi=50 --- D50 Total goodness of fit statistic at phi=50 --- Db40 Goodness of fit statistic for size-bend distributions at phi=40 --- Dq40 Goodness of fit statistic for size-Q distributions at phi=40 --- D40 Total goodness of fit statistic at phi=40 --- Db30 Goodness of fit statistic for size-bend distributions at phi=30 --- Dq30 Goodness of fit statistic for size-Q distributions at phi=30 --- D30 Total goodness of fit statistic at phi=30 --- Db20 Goodness of fit statistic for size-bend distributions at phi=20 --- Dq20 Goodness of fit statistic for size-Q distributions at phi=20 --- D20 Total goodness of fit statistic at phi=20 --- James Marcout, Patricia Bauer CDS 1997 May 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_427_125.xml Determining structure in molecular clouds. J/ApJ/428/693 J/ApJ/428/693 Rosette Nebula and Maddalena Cloud structures Determining structure in molecular clouds. J P Williams E J De Geus L Blitz Astrophys. J. 428 693 1994 1994ApJ...428..693W Morphology Nebulae ISM: individual (Rosette Nebula, Maddalena Cloud) ISM: structure methods: analytical stars: formation We describe an automatic, objective routine for analyzing the clumpy structure in a spectral line position-position-velocity data cube. The algorithm works by first contouring the data at a multiple of the rms noise of the observations, then searches for peaks of emission which locate the clumps, and then follows them down to lower intensities. No a priori clump profile is assumed. By creating simulated data, we test the performance of the algorithm and show that a contour map most accurately depicts internal structure at a contouring interval equal to twice the rms noise of the map. Blending of clump emission leads to small errors in mass and size determinations and in severe cases can result in a number of clumps being misidentified as a single unit, flattening the measured clump mass spectrum. The algorithm is applied to two real data sets as an example of its use. The Rosette molecular cloud is a "typical" star-forming cloud, but in the Maddalena molecular cloud high-mass star formation is completely absent. Comparison of the two clump lists generated by the algorithm show that on a one-to-one basis the clumps in the star-forming cloud have higher peak temperatures, higher average densities, and are more gravitationally bound than in the non star-forming cloud. Collective properties of the clumps, such as temperature-size-line-width-mass relations appear very similar, however. Contrary to the initial results reported in a previous paper (Williams & Blitz, 1993ApJ...405L..75W), we find that the current, more thoroughly tested analysis finds no significant difference in the clump mass spectrum of the two clouds.
Clumps in the Rosette molecular cloud RMC Clump number ([WDB94] RMC NN in Simbad) --- GLON Peak galactic longitude deg GLAT Peak galactic latitude deg Vpeak Peak velocity km/s Tpeak Peak temperature K DR Equivalent circular radius number=1 Data corrected for beam size as described in Appendix A pc FWHM Line width number=1 Data corrected for beam size as described in Appendix A km/s Mlte Clump masses number=2 Clump masses, derived from the integrated ^13^CO luminosity assuming LTE, {tau}_13_<0.5, N_H2_/N_^13^CO_=4.8x10^5^, and T_ex_=20K. Includes an additional factor of 1.4 for helium. solMass Mvir Virial mass number=3 Virial mass, assuming an inverse-square power-law density profile (see Appendix A) solMass Clumps in the Maddalena molecular cloud: region 1 (RA=6h46m50s, DE=-4{deg}31'14") Clumps in the Maddalena molecular cloud: region 2 (RA=6h43m39s, DE=-3{deg}30'23") MMC Clump number number=1 table3a.dat: [WDB94] MMC-1 NN in Simbad table3b.dat: [WDB94] MMC-2 NN in Simbad --- oRApeak Offset from right ascension number=2 For table3a.dat, RA=6h46m50s, DE=-4{deg}31'14" For table3b.dat, RA=6h43m39s, DE=-3{deg}30'23" arcmin oDEpeak Offset from declination number=2 For table3a.dat, RA=6h46m50s, DE=-4{deg}31'14" For table3b.dat, RA=6h43m39s, DE=-3{deg}30'23" arcmin Vpeak Peak velocity km/s Tpeak Peak temperature K DR Equivalent circular radius number=3 Data corrected for beam size as described in Appendix A pc FWHM Line width number=3 Data corrected for beam size as described in Appendix A km/s Mlte Clump masses number=4 Clump masses, derived from the integrated ^13^CO luminosity assuming LTE, {tau}_13_<0.5, N_H2_/N_^13^CO_=4.8x10^5^, and T_ex_=10K. Includes an additional factor of 1.4 for helium. solMass Mvir Virial mass number=5 Virial mass, assuming an inverse-square power-law density profile (see Appendix A) solMass James Marcout, Patricia Bauer CDS 1998 Oct 12 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_428_693.xml Physical structure of H2O masers in W49N J/ApJ/429/253 J/ApJ/429/253 W49N H2O masers Physical structure of H2O masers in W49N C R Gwinn Astrophys. J. 429 253 1994 1994ApJ...429..253G Masers Radio lines VLBI ISM: individual (W49) ISM: jets and outflows ISM: kinematics and dynamics ISM: molecules masers VLBI observations of a H2O maser were done at five epochs in 1980-82 with a 5 station VLBI network (see 1992ApJ...393..149G). A model was fitted to each peak in any spectral channel exceeding 5 times the rms background. The minimum level of this background, due to system noise at the antennas, was about 0.2Jy at each epoch. The model parameters include right ascension and declination offset (x, y) relative to a reference position; the total flux density, S; and the angular diameter {theta}_H_, of the best-fitting Gaussian distribution of intensity. The fitted parameters are in table1.
W 49N 19 10 13.1 +09 06 12
Features observed 1982 March 6 [G94] Sequential number --- oRA Right ascension offset from a reference position mas oDE Declination offset from a reference position mas Vz Doppler velocity km/s DVz Line width km/s Sp Peak flux density Jy Theta Angular size mas James Marcout, Patricia Bauer, CDS 1996 Aug 09 UNKNOWN UNKNOWN Scanned and processed via OCR at CDS. J_ApJ_429_253.xml A statistical analysis of the broadband 0.1 to 3.5keV spectral properties of X-ray-selected active galactic nuclei. J/ApJ/434/54 J/ApJ/434/54 Spectral properties of X-ray-selected AGNs A statistical analysis of the broadband 0.1 to 3.5keV spectral properties of X-ray-selected active galactic nuclei. R J Thompson F A Cordova Astrophys. J. 434 54 1994 1994ApJ...434...54T Active gal. nuclei X-ray sources galaxies: active X-rays: galaxies We survey the broadband spectral properties of ~500 X-ray-selected active galactic nuclei (AGNs) observed with the Einstein Observatory. Included in this survey are the ~450 AGNs in the Extended Medium Sensitivity Survey of Gioia et al. (1990ApJS...72..567G) and the ~50 AGNs in the Ultrasoft Survey of Cordova et al. (1992ApJS...81..661C). We present a revised version of the latter sample, based on the post publication discovery of a software error in the Einstein Rev-1b processing. We find that the mean spectral index of the AGNs between 0.1 and 0.6keV is softer, and the distribution of indices wider, than previous estimates based on analyses of the X-ray spectra of optically selected AGNs. A subset of these AGNs exhibit flux variability, some on timescales as short as 0.05-days. A correlation between radio and hard X-ray luminosity is confirmed, but the data do not support a correlation between the radio and soft X-ray luminosities, or between radio loudness and soft X-ray spectral slope. Evidence for physically distinct soft and hard X-ray components is found, along with the possibility of a bias in previous optically selected samples toward selection of AGNs with flatter X-ray spectra.
Revised Ultrasoft Survey (RUSS) Sources Name Source name --- n_Seq Note number=1 *: source that satisfy our criteria for being "truly" soft, i.e. being free from shadowing by the detector support ribs and having good counting statistics (R1 +1{sigma}<0.6) --- Seq IPC sequence --- SRC Source number --- RAXh X-ray right ascension (1950) h RAXm X-ray right ascension (1950) min RAXs X-ray right ascension (1950) s DEX- X-ray declination sign --- DEXd X-ray declination (1950) deg DEXm X-ray declination (1950) arcmin DEXs X-ray declination (1950) arcsec RAh Optical right ascension (1950) h RAm Optical right ascension (1950) min RAs Optical right ascension (1950) s DE- Optical declination sign --- DEd Optical declination (1950) deg DEm Optical declination (1950) arcmin DEs Optical declination (1950) arcsec z Redshift --- Vmag V magnitude mag NH Hydrogen column density 10+20cm-2 RECO IPC RECO value number=2 Measure of the amount of shadowing by the detector support ribs, Harnden et al., 1984, Smithsonian Astrophys. Obs. Spec. Rep. No. 393 --- Dits Off-axis distance arcmin RUSS X-Ray data Name Source name, as in table1a --- R1 Counts in colour ratio R1 --- e_R1 rms uncertainty on R1 --- R2 Counts in colour ratio R2 (C3/C2) --- e_R2 rms uncertainty on R2 --- C1 Counts ratio at the energy band C1=0.16-0.56keV --- e_C1 rms uncertainty on C1 --- C2 Counts ratio at the energy band C2=0.56-1.08keV --- e_C2 rms uncertainty on C2 --- C3 Counts ratio at the energy band C3=1.08-3.5keV --- e_C3 rms uncertainty on C3 --- RUSS X-ray luminosities Name Source name, as in table1a --- IPC IPC counts ct/s e_IPC rms uncertainty on IPC ct/s L1s Soft-component luminosity for the 10eV rest-frame model solLum L2s Soft-component luminosity for the 7.85eV observed-frame model solLum l_Lh Limit flag on Lh --- Lh Hard-component luminosity from the observer-frame model solLum L0.2keV Monochromatic 0.2keV luminosity solLum l_L2.0keV Limit flag on L2.0keV --- L2.0keV Monochromatic 2.0keV luminosity solLum James Marcout, Patricia Bauer CDS 1997 Jun 06 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_434_54.xml The complete Einstein Observatory X-ray survey of the Orion nebula region. J/ApJ/437/361 J/ApJ/437/361 Einstein survey of the Orion nebula region The complete Einstein Observatory X-ray survey of the Orion nebula region. M Gagne J -P Caillault Astrophys. J. 437 361 1994 1994ApJ...437..361G II/171 : Parenago Catalogue of stars in the area of the Orion Nebula (1954) II/36 : Photometry of Orion OB1 Association (Warren+ 1977) J/ApJ/445/280 : ROSAT survey of the Orion nebula region (Gagne+ 1995) Abt et al. 1991 ApJ 367, 155 =1991ApJ...367..155A Andrews 1981 "A Photometric atlas of the Orion Nebula" (Belfast: Armagh Obs. Press) Attridge & Herbst 1992 ApJ 398, L61 =1992ApJ...398L..61A Attridge & Herbst 1994, in prep. Brun 1935 Pub. Obs. Lyon, 1, No 12 =1935POLyo...1...12B Cohen & Kuhi 1979 ApJS 41, 743 =1979ApJS...41..743C Duncan 1993 ApJ 406, 172 =1993ApJ...406..172D Edwards et al. 1993 AJ 106, 372 =1993AJ....106..372E General Catalogue of Variable Stars =CDS Catalogue: <II/139> Hartmann et al. 1986 ApJ 309, 275 =1986ApJ...309..275H Herbig & Terndrup 1986 ApJ 307, 609 =1986ApJ...307..609H Herbst (1993) private comm. Jones & Walker 1988 AJ 95, 1755 =1988AJ.....95.1755J Mandel & Herbst 1991 ApJ 383, L75 =1991ApJ...383L..75M McNamara & Huels 1983 A&AS 54, 221 =1983A&AS...54..221M McNamara et al. 1989 AJ 97, 1427 =1989AJ.....97.1427M Parenago 1954 =CDS Catalogue: <II/171> Parsamian & Chavira 1982 Bol. Inst. Tonantzintla 3, 69 =1982BITon...3...69P Rydgren & Vrba 1984 AJ 89, 399 =1984AJ.....89..399R Smith et al. 1983 ApJ 271, 237 =1983ApJ...271..237S Smith et al. 1983 ApJ 272, 163 =1983ApJ...272..163S Strom 1993 private comm. Strom 1994 ApJ 424, 237 =1994ApJ...424..237S Strom et al. 1990 ApJ 362, 168 =1990ApJ...362..168S van Altena et al. 1988 AJ 95, 1744 =1988AJ.....95.1744V Walker 1969 ApJ 155, 447 =1969ApJ...155..447W Walker 1983 ApJ 271, 642 =1983ApJ...271..642W Walker 1990 PASP 102, 726 =1990PASP..102..726W Warren & Hesser 1977 ApJS 34, 115 =CDS Catalogue: <II/36> Nebulae X-ray sources stars: stars: pre-main sequence X-rays: stars We have analyzed archival Einstein Observatory images of a roughly 4.5 square degree region centered on the Orion Nebula. In all, 245 distinct X-ray sources have been detected in six High Resolution Imager (HRI) and 17 Imaging Proportional Counter (IPC) observations. An optical database of over 2700 stars has been assembled to search for candidate counterparts to the X-ray sources. Roughly half the X-ray sources are identified with a single Orion Nebula cluster member. The 10 main-sequence O6-B5 cluster stars detected in Orion have X-ray activity levels comparable to field O and B stars. X-ray emission has also been detected in the direction of four main-sequence late-B and early-A type stars. Since the mechanisms producing X-rays in late-type coronae and early-type winds cannot operate in the late-B and early-A type atmospheres, we argue that the observed X-rays, with L_X_~3x10^30^ergs/s, are probably produced in the coronae of unseen late-type binary companions. Over 100 X-ray sources have been associated with late-type pre-main sequence stars.
Einstein
Sources detected in the Orion Nebula Region by Einstein NoX X-ray number --- RAh Right ascension (J2000) of the source h RAm Right ascension (J2000) of the source min RAs Right ascension (J2000) of the source s DE- Declination sign --- DEd Declination (J2000) of the source deg DEm Declination (J2000) of the source arcmin DEs Declination (J2000) of the source arcsec Rate1 IPC count rate ct/s e_Rate1 rms uncertainty on Rate1 ct/s Rate2 HRI count rate ct/s e_Rate2 rms uncertainty on Rate2 ct/s DRA Offset in right ascension arcsec DDE Offset in declination arcsec Name Star name --- n_Name * indicates multiple optical counterpart. See table3 --- Prob Membership probability --- Einstein sources with multiple optical counterparts NoX X-ray number --- oRA1 Offset in right ascension for star1 arcsec oDE1 Offset in declination for star1 arcsec Star1 Star1 name --- Prob1 Membership probability for star1 --- oRA2 Offset in right ascension for star2 arcsec oDE2 Offset in declination for star2 arcsec Star2 Star2 name --- Prob2 Membership probability for star2 --- oRA3 Offset in right ascension for star3 arcsec oDE3 Offset in declination for star3 arcsec Star3 Star3 name --- Prob3 Membership probability for star3 --- Optical and X-ray data for typed cluster members NoX X-ray number --- Par Parenago (1954) designation --- J&W Jones & Walker (1988) designation --- GCVS GCVS designation --- Sp Spectral type --- lofTeff Effective temperature K Bmag B magnitude mag Vmag V magnitude mag Icmag Ic magnitude mag logLX X-ray luminosity 10-7J log(LX/Lbol) X-ray luminosity versus bolometric luminosity ratio --- Note Notes number=1 a: Position and proper-motion membership probability from McNamara et al. 1989 b: Position and proper-motion membership probability from Jones & Walker 1988 c: Position and proper-motion membership probability from van Altena et al. 1988 d: Proper-motion membership probability from McNamara & Huels 1983 e: Spectral type, V and Ic band photometry from Edwards et al. 1993 f: Spectral type from Strom 1993 g: Spectral type, B and V band photometry from Duncan 1993 h: Spectral type, V and Ic band photometry from Strom et al. 1990 i: Spectral type from Abt et al. 1991 j: Spectral type from van Altena et al. 1988 k: Spectral type from the General Catalogue of Variable Stars (Kholopov et al. 1985) l: Spectral type from Walker 1983 m: Spectral type from Smith et al. 1983 n: Spectral type and V band photometry from Cohen & Kuhi 1979 o: Spectral type from Warren & Hesser 1977 p: Spectral type, B and V band photometry from Walker 1969 q: Spectral type from Parenago 1954 r: V and Ic photometry from Attridge & Herbst 1992 or Herbst (1993) s: Position or spectral type, V and Ic band photometry from Herbig & Terndrup 1986 t: B and V band photometry from Duncan 1993 u: B and V band photometry from McNamara et al. 1989 v: B and V band photometry from van Altena et al. 1988 w: B, V, and Ic band photometry from Rydgren & Vrba 1984 x: B and V band photometry from Warren & Hesser 1977 y: Ic photometric magnitude from Jones & Walker 1988 z: Position, B and V photographic magnitude from Andrews 1981 A: Position, B and V photographic magnitude from Parsamian & Chavira 1982 B: V photographic magnitude from Brun 1935 C: The bolometric luminosity of the late-type secondary cannot be determined D: Position and V photovisual magnitude from Parenago 1954 --- Optical and X-ray data for untyped cluster members NoX X-ray number --- Par Parenago (1954) designation --- J&W Jones & Walker (1988) designation --- GCVS GCVS designation --- Bmag B magnitude mag Vmag V magnitude mag Icmag Ic magnitude mag logLX X-ray luminosity 10-7J n_logLX Note on LX number=1 JW 315 may have been flaring during HRI exposure (see table2). Consequently, we have used IPC count rate to determine LX. --- log(fX/fbol) X-ray flux versus bolometric flux ratio --- Note Notes number=2 Same as note (1) of table7 --- Rotational and X-ray data for late-type cluster members NoX X-ray number --- Par Parenago (1954) designation --- J&W Jones & Walker (1988) designation --- GCVS GCVS designation --- Sp Spectral type --- logLX X-ray luminosity 10-7J logFX X-ray flux mW/m2 u_logFX Uncertainty flag on logFX --- l_vsini Limit flag on vsini --- vsini Rotational velocity km/s Prot Period of rotation d Note Notes number=1 a: Rotational period from Attridge & Herbst 1994 b: Rotational period from Attridge & Herbst 1992 c: Rotational period from Mandel & Herbest 1991 d: Rotational period from Walker 1990 e: Spectroscopic rotational velocity from Strom 1994 f: Spectroscopic rotational velocity from Duncan 1993 g: Spectroscopic rotational velocity from Walker 1990 h: Spectroscopic rotational velocity from Hartmann et al. 1986 i: Spectroscopic rotational velocity from Smith et al. 1983 --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Aug 14 Marc Gagne <marc@charon.colorado.edu> J_ApJ_437_361.xml Ultraviolet Imaging Telescope and Optical Emission-Line Observations of H II Regions in M81 J/ApJ/438/181 J/ApJ/438/181 Observations of H II Regions in M81 Ultraviolet Imaging Telescope and Optical Emission-Line Observations of H II Regions in M81 J K Hill K -P Cheng R C Bohlin R H Cornett P M N Hintzen R W O'Connell M S Roberts A M Smith E P Smith T P Stecher Astrophys. J. 438 181 1995 1995ApJ...438..181H H II regions Ultraviolet dust, extinction galaxies: individual (M 81) galaxies: stellar content HII regions ultraviolet: galaxies Images of the type Sab spiral galaxy M81 were obtained in far-UV and near-UV bands by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission of 1990 December. Magnitudes in the two UV bands are determined for 52 H II regions from the catalog of Petit, Sivan, & Karachentsev (1988A&AS...74..475P). Fluxes of the H-alpha and H-beta emission lines are determined from CCD images. Extinctions for the brightest H II regions are determined from observed Balmer decrements. Fainter H II regions are assigned the average of published radio-H-alpha extinctions for several bright H II regions. The radiative transfer models of Witt, Thronson, & Capuano (1992, ApJ, 393, 611) are shown to predict a relationship between Balmer Decrement and H-alpha extinction consistent with observed line and radio fluxes for the brightest 7 H II regions and are used to estimate the UV extinction. Ratios of Lyman continuum flux (computed from the extinction corrected H-alpha flux) to the extinction corrected far-UV flux are compared with ratios predicted by model spectra computed for IMF slope equal to -1.0 and stellar masses ranging from 5 to 120 Msun. Ages and masses are estimated by comparing the H-alpha and far-UV fluxes and their ratio with the models. The total of the estimated stellar masses for the 52 H II regions is 1.4x10^5^ Msun. The star-formation rate inferred for M81 from the observed UV and H-alpha fluxes is low for a spiral galaxy at ~0.13 Msun/yr, but consistent with the low star-formation rates obtained by Kennicutt (1983ApJ...272...54K) and Caldwell et al. (1991ApJ...370..526C) for early-type spirals.
M81 H II region photometry PSK H II region number from PSK H II region number from Petit, Sivan, & Karachentsev (1988A&AS...74..475P) --- m152 Far-UV magnitude mag e_m152 Estimated error in m152 mag m249 Near-UV magnitude mag e_m249 Estimated error in m249 mag fHa H-alpha flux 10-14mW/m2 e_fHa Estimated fractional error in fHa 10-14mW/m2 fHb H-beta flux For 11 H II regions not measurable in the H-beta line, the H-beta fluxes and the corresponding errors are both set to 0.0. 10-14mW/m2 e_fHb Estimated fractional error in fHb 10-14mW/m2 table2.tex LaTeX version of Table 2 environ.tex Custom LaTeX environments and related macros CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 06-May-1995 J_ApJ_438_181.xml Correlations between the flaring radio emission and starspot distribution of UX Arietis J/ApJ/439/983 J/ApJ/439/983 Radio & optical observation of UX Arietis Correlations between the flaring radio emission and starspot distribution of UX Arietis N M Elias II A Quirrenbach A Witzel C E Naundorf R Wegner E F Guinan G P McCook Astrophys. J. 439 983 1995 1995ApJ...439..983E Photometry Radio lines Stars, flare radio continuum: stars stars: flare stars: individual (UX Arietis) We have observed UX Arietis at C band (6cm) for 3 weeks with four VLA antennas. The temporal coverage during the program was approximately three scans per day. A few days into the VLA program, UX Ari began a radio flaring period which lasted for at least 2 weeks. All the radio fluxes were above the system noise during this episode, but the largest values (up to 270mJy) occurred close to 0.0 phase. This phasing is confirmed by the UX Ari radio observations of Neidhoefer, Massi, & Chiuderi-Drago (1993A&A...278L..51N). Visible-band light curves of UX Ari were obtained both during and after our radio observations; the peak-to-peak variation in all filters was ~0.2mag. The light curves indicate that the maximum starspot visibility occurred very close to 0.0 phase, the same phase as the radio maxima. Closer comparison of our radio and optical light curves indicates that they are almost perfectly anticorrelated. A similar radio/optical correlation has been found by Lim et al. (1992ApJ...388L..27L) and Lim et al. (1994ApJ...430..332L) for the single K0 V star AB Dor. We make the following conclusions from our observations. First, the episodes of long-term (~hours to days) radio flaring were modulated by stellar eclipses. Second, the flares were located close to the starspot groups. Third, the sizes of the flares were comparable to sizes of the starspot groups, which is consistent with nonthermal emission of brightness temperature T_b~10^10-10^13K. Fourth, the radio emission arose only from the midlatitude starspot groups. Last, the radio flares emitted their radiation nearly normal to the stellar surface.
UX Ari HD 21242 03 26 35.1 +28 42 59
UX Arietis C-band VLA observations HJD Heliocentric Julian Date d Phase Phase --- Flux Radio flux mJy UX Arietis visible-band photometry HJD Heliocentric Julian Date d Phase Phase --- dMag Differential magnitude, Var - Comp Comparison star was 62 Ari (HR 1012, HD 20825; V=+5.52; B-V=+1.10; G5 III). Check star was HR 999 (HD 20644, V=+4.47, B-V=+1.54; K4 III). 62 Ari has been used previously in photometric studies of UX Ari and appears to be constant in light. mag Filter Filter: b', y, r Intermediate-band interference filters: b' - lambda = 453nm, FWHM = 15nm y - Stroemgren y, lambda = 550nm, FWHM = 35nm r - lambda = 660nm, FWHM = 28nm, also known as H-alpha I --- Obs Observatory, VUO or APT VUO - Villanova University Observatory, APT - Automatic Photometric Telescope, Mount Hopkins, Arizona --- CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 06-May-1995 J_ApJ_439_983.xml The deceleration powering of synchrotron emission from ejecta components in supernova remnant Cassiopeia A J/ApJ/441/307 J/ApJ/441/307 Proper motions and brightness of Cas A The deceleration powering of synchrotron emission from ejecta components in supernova remnant Cassiopeia A M C Anderson L Rudnick Astrophys. J. 441 307 1995 1995ApJ...441..307A Proper motions Radio sources Supernova remnants ISM: individual (Cas A) ISM: kinematics and dynamics ISM: structure supernova remnants techniques: interferometric The results of a multiple-epoch radio study of secular changes in the SNR Cassiopeia A are reported and used to construct a model for the dynamical evolution of diffuse and clumpy ejecta components in the remnant. To quantify the current dynamical status of various ejecta components, the proper motions and brightness evolution of a sample of 304 compact radio features have been accurately determined from high-quality interferometric observations of the remnant at lambda=6 and 20cm, spanning a total time baseline of 12yr. A simple model of homologous expansion does not provide a good fit to the measured proper motions of the radio knots. We find that a single estimate of the ejecta expansion age is not appropriate, as the expansion derived from compact features varies azimuthally and radially in the remnant and differs for subsets of knots segregated by brightness. We verify that the bulk of the radio-emitting plasma in Cas A has indeed been significantly decelerated by the current epoch; bulk expansion ages of 2.5-4 times the actual age of the remnant are measured . Based on these dynamical data, and information on the kinematics of the fast moving optical knots. we synthesize a model that directly relates the dynamics of ejecta components in Cas A to various radiative processes. This model is based on the premise that the emission from Cas A, at a variety of wavelengths, is deceleration-powered. If ejecta components are distributed over a range of internal densities, a sequential "turning-on" of components, in order of increasing density, should be observed. A model for the current emission distribution in Cas A, at radio, X-ray, and optical wavelengths, is outlined in terms of deceleration considerations.
Cas A SNR 111.7-02.1 23 23 12.6 +58 48 48
Results of multi-epoch fits Knot Knot designation number. --- KnotT Designation number of Tuffs (1986MNRAS.219...13T), for knots which are clearly in both samples. --- Xpos Epoch 1987 knot position number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) arcsec Ypos Epoch 1987 knot position number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) arcsec BoxX1 Box defining the regression region used for each knot number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) arcsec BoxY1 Box defining the regression region used for each knot number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) arcsec BoxX2 Box defining the regression region used for each knot number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) arcsec BoxY2 Box defining the regression region used for each knot number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) arcsec pmRA Proper motion in right ascension arcsec/yr e_pmRA rms uncertainty in pmRA (68% confidence) arcsec/yr pmDE Proper motion in declination arcsec/yr e_pmDE rms uncertainty in pmDE (68% confidence) arcsec/yr B Estimate of knot brightness at lambda=6cm (mJy/beam, epoch 1987) mJy DB/B Annual fractional brightness change relative to the large-scale ring yr-1 e_DB/B rms uncertainty in DB/B (68% confidence) yr-1 Nobs Number of epochs of data used in multi-epoch determinations --- James Marcout, Patricia Bauer CDS 1996 Oct 02 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_441_307.xml A Multiparametric Analysis of the Einstein Sample of Early-Type Galaxies. II. Galaxy Formation History and Properties of the Interstellar Medium J/ApJ/442/523 J/ApJ/442/523 Multiparam. Analysis, Einstein Sample. II. A Multiparametric Analysis of the Einstein Sample of Early-Type Galaxies. II. Galaxy Formation History and Properties of the Interstellar Medium P B Eskridge G Fabbiano D -W Kim Astrophys. J. 442 523 1995 1995ApJ...442..523E galaxies: elliptical and lenticular, cD galaxies: ISM We have conducted bivariate and multivariate statistical analysis of data measuring the integrated luminosity, shape, and potential depth of the Einstein sample of early-type galaxies (presented by Fabbiano et al. =1992ApJS...80..531F). We find significant correlations between the X-ray properties and the axial ratios (a/b) of our sample, such that the roundest systems tend to have the highest L_X and L_X/L_B. The most radio-loud objects are also the roundest. We confirm the assertion of Bender et al. (1989A&A...217...35B) that galaxies with high L_X are boxy (have negative a_4). Both a/b and a_4 are correlated with L_B, but not with IRAS 12 um and 100 um luminosities. There are strong correlations between L_X, Mg_2 and sigma_v in the sense that those systems with the deepest potential wells have the highest L_X and Mg_2. Thus the depth of the potential well appears to govern both the ability to retain an ISM at the present epoch and to retain the enriched ejecta of early star formation bursts. Both L_X/L_B and L_6 (the 6 cm radio luminosity) show threshold effects with sigma_v, exhibiting sharp increases at log(sigma_v) ~ 2.2. Finally, there is clearly an interrelationship between the various stellar and structural parameters: The scatter in the bivariate relationships between the shape parameters (a/b and a_4) and the depth parameter (sigma_v) is a function of abundance in the sense that, for a given a_4 or a/b, the systems with the highest sigma_v also have the highest Mg_2. Furthermore, for a constant sigma_v, disky galaxies tend to have higher Mg_2 than boxy ones. Alternatively, for a given abundance, boxy ellipticals tend to be more massive than disky ellipticals. One possibility is that early-type galaxies of a given mass, originating from mergers (boxy ellipticals), have lower abundances than "primordial" (disky) early-type galaxies. Another is that disky inner isophotes are due not to primordial dissipational collapse, but to either the self-gravitating inner disks of captured spirals or the dissipational collapse of new disk structures from the premerger ISM. The high measured nuclear Mg_2 values would thus be due to enrichment from secondary bursts of star formation triggered by the merging event.
Partial Spearman Rank Analysis: Trends with Log(a/b), E+S0 Sample Pair Test pair, if blank, record is a continuation --- Held Quantities to be held constant in the test --- Size Number of objects in the sample --- Spearman Partial Spearman rank statistic --- l_Prob Probability limiting character --- Prob Probability that the test pair shows a correlation for this set of parameters --- Partial Spearman Rank Analysis: Trends with Log(a/b), Separate E and S0 Samples Pair Test pair, if blank, record is a continuation --- Held Quantities to be held constant in the test --- Sample Sample designation, Es or S0s --- Size Number of objects in the sample --- Spearman Partial Spearman rank statistic --- l_Prob Probability limiting character --- Prob Probability that the test pair shows a correlation for this set of parameters --- Partial Spearman Rank Analysis: Trends with Mg_2 Pair Test pair, if blank, record is a continuation --- Held Quantities to be held constant in the test --- Size Number of objects in the sample --- Spearman Partial Spearman rank statistic --- l_Prob Probability limiting character --- Prob Probability that the test pair shows a correlation for this set of parameters --- Partial Spearman Rank Analysis: Trends with sigma_v Pair Test pair, if blank, record is a continuation --- Held Quantities to be held constant in the test --- Size Number of objects in the sample --- Spearman Partial Spearman rank statistic --- l_Prob Probability limiting character --- Prob Probability that the test pair shows a correlation for this set of parameters --- Partial Spearman Rank Analysis: Trends with a_4 Pair Test pair, if blank, record is a continuation --- Held Quantities to be held constant in the test --- Size Number of objects in the sample --- Spearman Partial Spearman rank statistic --- l_Prob Probability limiting character --- Prob Probability that the test pair shows a correlation for this set of parameters --- CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 06-May-1995 J_ApJ_442_523.xml Radial Velocities of Stars in the Globular Cluster M4 and the Cluster Distance J/ApJ/443/124 J/ApJ/443/124 Radial Velocities of Stars in M4 Radial Velocities of Stars in the Globular Cluster M4 and the Cluster Distance R C Peterson R F Rees K M Cudworth Astrophys. J. 443 124 1995 1995ApJ...443..124P globular clusters: individual (M 4) stars: kinematics techniques: radial velocities The internal stellar velocity distribution of the globular cluster M4 is evaluated from nearly 200 new radial velocity measurements good to 1 km/s and a rederivation of existing proper motions. The mean radial velocity of the cluster is 70.9 +/- 0.6 km/s. The velocity dispersion is 3.5 +/- 0.3 km/s at the core, dropping marginally towards the outskirts. Such a low internal dispersion is somewhat at odds with the cluster's orbit, for which the perigalacticon is sufficiently close to the galactic center that the probability of cluster disruption is high; a tidal radius two-thirds the currently accepted value would eliminate the discrepancy. The cluster mass-to-light ratio is also small, M/L_V = 1.0 +/- 0.4 in solar units. M4 thus joins M22 as a cluster of moderate mass and concentration with a mass-to-light ratio among the lowest known. The astrometric distance to the cluster is also smaller than expected, 1.72 +/- 0.14 kpc. This is only consistent with conventional estimates of the luminosity of horizontal branch stars provided an extinction law R = A_V/E(B-V) ~ 4 is adopted, as has been suggested recently by several authors.
Velocities for M4 members RAh Right ascension (equinox 1950.0) h RAm R.A. min RAs R.A. s DE- Declination sign --- DEd Declination (equinox 1950.0) deg DEm Dec. arcmin DEs Dec. arcsec Dist Radial distance from cluster center arcmin PA Position angle positive north through east deg Vmag V magnitude mag B-V B-V color mag Date Julian date of each observation Julian date of each observation, or that of the first observation if the star was observed twice or more. d RV Measured radial velocity For all multiply observed stars, this is the weighted mean of the set of observations in Table 3. km/s e_RV Internal uncertainty in RV The uncertainty is derived from the ratio R of the height of the cross-correlation peak relative to a typical noise fluctuation, according to the Tonry & Davis [1979, AJ, 84, 1511] formula sigma_R = K/(1+R) (in km/s), with K=8.3 for sharp-lined spectra obtained with the Mount Hopkins echelle spectrographs. km/s Memb =-1 Percent probability of membership % ID Identification Star Name: Lee (1977, A&AS, 27, 367) number, no prefix; Sawyer-Hogg (1973, Pub. DDO, 3, No. 6) variable, prefix V; Alcaino (1975, A&AS, 21, 5) single letter or prefix A; Greenstein (1939, ApJ, 90, 387) prefix G --- *Velocities for M4 nonmembers RAh Right ascension (equinox 1950.0) h RAm R.A. min RAs R.A. s DE- Declination sign --- DEd Declination (equinox 1950.0) deg DEm Dec. arcmin DEs Dec. arcsec Dist Radial distance from cluster center arcmin PA Position angle positive north through east deg Vmag V magnitude mag B-V B-V color mag Date Julian date of each observation d RV Measured radial velocity km/s e_RV Internal uncertainty in RV km/s Memb Percent probability of membership % ID Identification --- Duplicate velocities Date Julian date of each observation d RV Measured radial velocity km/s e_RV Internal uncertainty in RV km/s ID Number from Lee 1977, A&AS, 27, 367 --- Proper-motion data superseding Table 3 of Cudworth & Rees =1990AJ.....99.1491C Names Star names Lee (1977, A&AS, 27, 367) number, no prefix; Sawyer-Hogg (1973, Pub. DDO, 3, No. 6) variable, prefix V; Alcaino (1975, A&AS, 21 5), single letter or prefix A; Alcaino and Liller (1984), AL -- second number is ring number; Zinn et al. (1972) UV-bright star, Z; Greenstein (1939, ApJ, 90, 387), prefix G --- X X coordinate relative to cluster center X and Y coordinates (arcsec) relative to the cluster center of Shawl and White (1986, AJ, 91, 312) and oriented along right ascension and declination for equator and equinox 1950 arcsec Y Y coordinate relative to cluster center arcsec mu_x Relative proper motion in X coordinate 0.01mas/yr e_mu_x Standard error in mu_x 0.01mas/yr mu_y Relative proper motion in Y coordinate 0.01mas/yr e_mu_y Standard error in mu_y 0.01mas/yr Vmag V magnitude mag B-V B-V color mag Pr Probability of membership based on relative proper motion % CDS 1995 Jul 11 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 06-May-1995 UNKNOWN UNKNOWN the Julian Dates were converted to absolute scale (initially with offset 2440000) J_ApJ_443_124.xml Deep ROSAT HRI observations of the Orion nebula region. J/ApJ/445/280 J/ApJ/445/280 ROSAT survey of the Orion nebula region Deep ROSAT HRI observations of the Orion nebula region. M Gagne J -P Caillault J R Stauffer Astrophys. J. 445 280 1995 1995ApJ...445..280G II/171 : Parenago catalogue in the area of the Orion nebula (1954) II/36 : UBV & uvby-beta obs. of Orion OB1 Association (Warren+ 1977) J/ApJ/437/361 : Einstein survey of the Orion nebula region (Gagne+ 1994) Abt et al. 1991 ApJ 367, 155 =1991ApJ...367..155A Andrews 1981 A Photometric atlas of the Orion Nebula (Belfadt: Armagh Obs. Press) Attridge & Herbst 1992 ApJ 398, L61 =1992ApJ...398L..61A Attridge & Herbst 1994, in prep. Brun 1935 Pub. Obs. Lyon, 1, No 12 =1935POLyo...1...12B Cohen & Kuhi 1979 ApJS 41, 743 =1979ApJS...41..743C Duncan 1993 ApJ 406, 172 =1993ApJ...406..172D Edwards et al. 1993 AJ 106, 372 =1993AJ....106..372E General Catalogue of Variable Stars =CDS Catalogue: <II/139> Hartmann et al. 1986 ApJ 309, 275 =1986ApJ...309..275H Herbig & Terndrup 1986 ApJ 307, 609 =1986ApJ...307..609H Jones & Walker 1988 AJ 95, 1755 =1988AJ.....95.1755J Mandel & Herbst 1991 ApJ 383, L75 =1991ApJ...383L..75M McNamara & Huels 1983 A&AS 54, 221 =1983A&AS...54..221M McNamara et al. 1989 AJ 97, 1427 =1989AJ.....97.1427M Parenago 1954 =CDS Catalogue: <II/171> Penston 1973, ApJ 183, 505 =1973ApJ...183..505P Penston et al. 1975, MNRAS 171, 219 =1975MNRAS.171..219P Prosser et al. 1994, ApJ 421, 517 =1994ApJ...421..517P Rydgren & Vrba 1984 AJ 89, 399 =1984AJ.....89..399R Strom 1993 private comm. van Altena et al. 1988 AJ 95, 1744 =1988AJ.....95.1744V Walker 1969 ApJ 155, 447 =1969ApJ...155..447W Walker 1983 ApJ 271, 642 =1983ApJ...271..642W Walker 1990 PASP 102, 726 =1990PASP..102..726W Warren & Hesser 1977 ApJS 34, 115 =CDS Catalogue: <II/36> Nebulae X-ray sources ISM: individual (Orion Nebula) stars: pre-main sequence X-rays: stars We present results from three deep ROSAT high-resolution imager observations of the Orion Nebula star-forming region. The X-ray images contain over 1500 catalogued stars in a roughly 0.8deg^2^ region centered on the Trapezium. In all, 389 distinct X-ray sources have been detected, at least two-thirds of which are associated with a single proper-motion cluster member. X-ray emission is detected from stars of all spectral types, from the massive O- and B-type components of the Trapezium to the coolest, low-mass pre-main-sequence (PMS) stars. In this paper, we focus primarily on X-ray emission from the late-type PMS stars. Of the ~100 late-type cluster members with measured spectral types, approximately three-fourths have been detected; we have derived X-ray luminosity upper limits for the remaining stars. We found coronal X-ray emission turns on around spectral type F6, with the upper envelope of activity increasing with decreasing effective temperature.
ROSAT
Orion Nebula X-ray sources NoX X-ray number --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec Count Corrected ROSAT HRI count rate ct/s e_Count rms uncertainty on Count ct/s Mult * indicates multiple candidate optical counterparts. See table3 --- Par Parenago (1954) optical counterpart candidate designation --- J&W Jones & Walker (1988) optical counterpart candidate designation --- Var Variable optical counterpart candidate designation --- Prob Membership probability --- DRA Offset in right ascension arcsec DDE Offset in declination arcsec X-ray sources with multiple candidate optical counterparts NoX X-ray number --- Par1 Parenago designation of the first candidate --- J&W1 Jones & Walker (1988) name of the first candidate --- Prob1 Membership probability of the first candidate --- DRA1 Offset in right ascension of the first candidate arcsec DDE1 Offset in declination of the first candidate arcsec Par2 Parenago designation of the second candidate --- J&W2 Jones & Walker (1988) name of the second candidate --- Prob2 Membership probability of the second candidate --- DRA2 Offset in right ascension of the second candidate arcsec DDE2 Offset in declination of the second candidate arcsec Par3 Parenago designation of the third third candidate --- J&W3 Jones & Walker (1988) name of the third candidate --- Prob3 Membership probability of the third candidate --- DRA3 Offset in right ascension of the third candidate arcsec DDE3 Offset in declination of the first candidate arcsec Optical and X-ray data for Group 1 stars Name Star name --- NoX X-ray number --- Sp Spectral type --- logTeff Effective temperature K u_logTeff Uncertainty flag on logTeff --- Bmag B magnitude mag Vmag V magnitude mag Icmag Ic (Cousins system) magnitude mag AV Visual extinction number=1 When accurate absorption values are available from published estimates, photometric E(B-V) measurements, or the C_Hbeta_ extinction map of the nebula, they are listed in this column. Otherwise we assume moderate absorption (A_V_~0.25mag) and indicate the value with a ')' in column n_AV mag n_AV ')' when AV=0.25mag number=1 When accurate absorption values are available from published estimates, photometric E(B-V) measurements, or the C_Hbeta_ extinction map of the nebula, they are listed in this column. Otherwise we assume moderate absorption (A_V_~0.25mag) and indicate the value with a ')' in column n_AV --- l_vsini Limit flag on vsini --- vsini Spectroscopic rotation velocity km/s Prot Rotational period d l_logLX Limit flag on logLX --- logLX X-ray luminosity 10-7J l_logLX/Lbol Limit flag on logLX/Lbol --- logLX/Lbol X-ray luminosity versus bolometric luminosity --- u_logLX/Lbol Uncertainty flag on logLX/Lbol --- Note Notes number=2 a: Position and proper-motion membership probability from McNamara et al. (1989) b: Position and proper-motion membership probability from Jones & Walker (1988) c: Position and proper-motion membership probability from van Altena et al. (1988) d: Proper-motion membership probability from McNamara & Huels (1983) e: Spectral type, V and Ic band photometry from Edwards et al. (1993) f: Spectral type from Strom (1993) g: Spectral type, B and V band photometry from Duncan (1993) h: Spectral type from Abt, Wang, & Cardona (1991) i: Spectral type from van Altena et al. (1988) j: Spectral type from the General Catalogue of Variable Stars (Kholopov et al. 1985) k: Spectral type from Walker (1983) l: Spectral type, B or V band photometry from Penston et al. (1975) or Penston (1973) m: Spectral type and V band photometry from Cohen & Kuhi (1979) n: Spectral type from Warren & Hesser (1977) o: Spectral type, B and V band photometry from Walker (1969) p: Spectral type from Parenago (1954) q: V and I_c_ band photometry from Prosser et al. (1994) r: V and I_c_ band photometry from Attridge & Herbst (1992) s: Position or spectral type, V and I_c_ band photometry from Herbig & Terndrup (1986) t: B and V band photometry from Duncan (1993) u: B and V band photometry from McNamara et al. (1989) v: B and V band photometry from van Altena et al. (1988) w: B, V, and I_c_ band photometry from Rydgren & Vrba (1984) x: B and V band photometry from Warren & Hesser (1977) y: I_c_ photographic magnitude from Jones & Walker (1988) z: Position, B and V photographic magnitudes from Andrews (1981) A: V photographic magnitude from Brun (1935) B: Position, B photographic or V photovisual magnitude from Parenago (1954) C: The bolometric luminosity of the late-type secondary cannot be determined D: Rotational period from Attridge & Herbst (1994) E: Rotational period from Attridge & Herbst (1992) F: Rotational period from Mandel & Herbst (1991) G: Rotational period from Walker (1990) H: Spectroscopic rotational velocity from Strom (1993) I: Spectroscopic rotational velocity from Duncan (1993) J: Spectroscopic rotational velocity from Abt et al. (1991) K: Spectroscopic rotational velocity from Walker (1990) L: Spectroscopic rotational velocity from Hartmann et al. (1986) M: One of two candidate optical counterparts. Upper limit corresponds to source flux N: Possible blend. Upper limit corresponds to half of source flux --- table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 table6.tex LaTeX version of table6 Patricia Bauer CDS 1996 Aug 19 Marc Gagne <marc@casa.Colorado.EDU> J_ApJ_445_280.xml Radio properties of optically selected quasars. J/ApJ/445/62 J/ApJ/445/62 Radio properties of optically selected quasars Radio properties of optically selected quasars. E J Hooper C D Impey C B Foltz P C Hewett Astrophys. J. 445 62 1995 1995ApJ...445...62H QSOs Radio sources Redshifts quasars: general radio continuum: galaxies surveys Approximately one-quarter (256 objects) of the Large Bright Quasar Survey (LBQS, Hewett et al., 1995, Cat. <J/AJ/109/1498>) has been observed with the VLA at 8.4GHz, resulting in 44 detections (17%) with a median 3{sigma} noise limit of 0.29mJy. Quasars with radio luminosity detectable at this limit are under-represented at faint absolute blue magnitudes (M_B_>=-24), an effect which cannot be explained by a potential LBQS selection bias against quasars which have large radio luminosities and small optical luminosities. The radio-loud (8GHz luminosity >10^25^W/Hz) fraction is observed to change as a function of redshift and MB, for M_B_<-24, although the causal variable is ambiguous. The description most consistent with the available data is that radio-loud fraction is approximately constant over the range -27.5<M_B_<-24 and increases at brighter absolute magnitudes. The radio-loud fraction as a function of redshift reaches a local maximum at z~1, and, aside from the effects of increased radio-loud fraction at bright M_B_, remains roughly constant to redshifts approaching 5. The log R_8.4_ distribution (radio-to-optical luminosity ratio) of the current LBQS sample may be bimodal, but the results of statistical tests are ambiguous, requiring a larger sample size to become definite.
Radio and optical observations of LBQS quasars LBQS Source name --- Bmag B magnitude mag z Redshift --- BMag Absolute B magnitude mag e_BMag rms uncertainty on BMag mag l_S8.4GHz Limit flag on S8.4GHz --- S8.4GHz Flux density at 8.4GHz mJy e_S8.4GHz rms uncertainty on S8.4GHz mJy l_logLr/Lb Limit flag on logLr/Lb --- logLr/Lb Ratio of 8.4GHz luminosity to optical luminosity averaged over the B passband --- e_logLr/Lb rms uncertainty on logLr/Lb --- l_logLr Limit flag on logLr --- logLr Luminosity at 8.4GHz [W/Hz] e_logLr rms uncertainty on logLr [W/Hz] James Marcout, Patricia Bauer CDS 1997 Jul 25 UNKNOWN UNKNOWN * 25-Jul-1997: prepared via OCR at CDS. * 04-Jun-1988: two OCR errors where corrected, thanks to H. Andernach <heinz@astro.ugto.mx> J_ApJ_445_62.xml Deep optical counterpart searches of gamma-ray burst localizations J/ApJ/446/115 J/ApJ/446/115 Gamma ray burst localizations Deep optical counterpart searches of gamma-ray burst localizations F J Vrba D H Hartmann M C Jennings Astrophys. J. 446 115 1995 1995ApJ...446..115V Gamma rays QSOs gamma rays: bursts quasars: general surveys techniques: photometric We report the results of a 5 year CCD imaging program of small gamma-ray burst (GRB) error boxes from the First Interplanetary Network and an optical transient field. The fields include GBS 0010-16, GBS 0552-08, GBS 1028+46, GBS 1205+23, GBS 1412+79, OTS 1809+31, GBS 2006-22, and GBS 2252-03. A total of 274 hours of open shutter time was used to obtain multiple UBVI-filtered frames covering an area approximately twice that of the 99% confidence localizations. For 2070 objects in these fields above the survey detection limit of V~24, 79,000 calibrated photometric measurements were made. The objectives of the survey were to search for objects of unusual colors, variability, or proper motions. The final census of objects in these fields is consistent with the expected numbers of normal stars, galaxies, and proper motion objects based on statistics of large-scale surveys. While no obvious GRB optical counterparts were found, several potentially interesting objects were discovered, along with marginal evidence for a QSO excess at the rate of one per high Galactic latitude localization. The results and implications are discussed in detail along with suggestions for future work.
Condensed Database Field Field name Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. --- Object Object identification number Object identification numbers for each field are arranged in decreasing order of declination. number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. --- Gal Indicates if object is a resolved galaxy number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. --- Vmag =-9.000 Mean V magnitude number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag e_Vmag =-1.000 Uncertainty in Vmag The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag B-V =-9.000 Mean (B-V) color number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag e_B-V =-1.000 Uncertainty in B-V number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag U-B =-9.000 Mean (U-B) color number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag e_U-B =-1.000 Uncertainty of U-B number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag V-I =-9.000 Mean (V-I) color number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag e_V-I =-1.000 Uncertainty in V-I number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag U-V =-9.000 Mean (U-V) color number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag e_U-V =-1.000 Uncertainty in U-V number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. mag Xpos X pixel coordinate The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. pix Ypos Y pixel coordinate number= Eight GBS or OTS fields are arranged in increasing order of Galactic latitude. The field name is repeated here for each object. number= Object identification numbers for each field are arranged in decreasing order of declination. number= The uncertainties listed are the larger of i) the weighted standard deviation of the mean, or ii) the minimum error based on the photometric uncertainties of individual observations. Thus, the listed error represents the uncertainty of the value whether primarily due to photometric error or variability. A -9.000 or -1.000 in the color/magnitude and uncertainty columns, respectively, indicates that there are insufficient data to calculate that quantity. A few lines of data are listed to only .01mag precision. These are highly extended objects whose photometric data were obtained by synthetic aperture photometry, rather than the usual point spread function fitting, as described in the text of the printed paper. number= The fiducial pixel coordinates (X,Y, with the origin at the northeast corner of each field) for each object to the nearest .01 pixel. Most pixel coordinates are from the Daophot `find' routine and have internal precisions of .01 pixel for the best exposed objects to about 1.0 pixel for the faintest and/or extended objects. Additionally, those objects with all zeros to the right of the decimal point for both X and Y were added to the object list by hand and have internal precisions of only 1.0 pixel. There was no attempt to estimate the internal precisions for each object since, as explained in Section 2.7 of the printed paper, the positional errors are dominated by not knowing the CCD rotation to better than about 0.5 degree. For an object lying 400 pixels from the center of the field this amounts to a 3.5 pixel error. At the telescope scale of 0.4295 arcsec/pixel the combined errors could be as large as 2 arcsec. Thus, the pixel coordinates should be used for identification purposes only and not for high accuracy astrometry. Finally, there are three objects (one each in the fields OTS 1809+31, GBS 2006-22, GBS 1205+23) with blank fields in X and Y. These are due to CCD artifacts which were realized as such only until well after the final object numbering system was finalized. pix Objects of possible interest Field Field name (Gamma Burst Source) --- No Object number --- o_Umag Number of observation in U filter --- o_Bmag Number of observation in B filter --- o_Vmag Number of observation in V filter --- o_Imag Number of observation in I filter --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag U-B U-B colour index mag e_U-B rms uncertainty on U-B mag V-I V-I colour index mag e_V-I rms uncertainty on V-I mag GRBBox This column answers whether the object lies within the IPN 99% confidence localization number=1 NA = not associated; IPN: Cline et al., 1980ApJ...237L...1C --- Dist Approximate distance to the nearest edge of the localization for objects that lies outside the localization. arcmin Com Comments number=1 NA = not associated; IPN: Cline et al., 1980ApJ...237L...1C --- UNKNOWN 1997 Jan 08 UNKNOWN UNKNOWN * 07-Oct-1995: AAS CD-ROM series, Volume 5, 1995 (Lee Brotzman [ADS]) * 12-Nov-1996: table6 added at CDS. J_ApJ_446_115.xml Neural network classification of the near-infrared spectra of A-type stars J/ApJ/446/300 J/ApJ/446/300 Classification of NIR spectra of A Stars Neural network classification of the near-infrared spectra of A-type stars W B Weaver A V Torres-Dodgen Astrophys. J. 446 300 1995 1995ApJ...446..300W III/181 : Near Infrared Spectra of Normal Stars (Torres-Dodgen+ 1993) Spectrophotometry Stars, A-type atlases dust, extinction infrared: stars stars: fundamental parameters techniques: spectroscopic The tables contain the flux data used to make figures 1-5 in the printed paper. The units of the flux columns are log(F_lambda), F_lambda in mW/m2/(0.1nm). Field labels for the flux values are keyed to the spectral type, in accordance with the labels in the figures. When fluxes are given for more than one star of a given type, a trailing "1", "2", etc. are appended to the label, however, this is not part of the spectral type. The star identification is given in the "Explanations." We present an atlas of near-infrared (NIR) spectra of A stars for luminosity classes Ia through V in the 15 A resolution system described by Torres-Dodgen and Weaver 1993 <III/181> and demonstrate an accurate method to automatically classify A stars on this system. Using equivalent widths, artificial neural networks (ANNs) can classify these spectra to an accuracy of 0.4 types (subclasses) in temperature and 0.15 classes in luminosity. Using the spectrum, with no manual intervention except wavelength registration, ANNs can classify these spectra with an accuracy comparable to that of 2A resolution MK classification: 0.5 types in temperature and 0.35 classes in luminosity. In addition, ANNs can concurrently determine reddening to an accuracy of 0.05 in E(B-V). We demonstrate that this NIR-ANN spectral classification system has the primary properties needed for automated classification surveys: it is based in the most efficient spectral region of modern silicon-based detectors, it requires low resolution (15A) spectra to achieve sub-classification box accuracy, it can produce two dimensional classifications at least as accurate as those by expert human classifiers, it is relatively insensitive to interstellar reddening and can accurately determine the reddening, it can identify and classify composite spectra, it degrades slowly with decreasing signal-to-noise ratio, and it requires a minimum of human interaction at all stages of the process.
HR 4554 HD 103287 11 53 49.2 +53 41 40 HR 7001 HD 172167 Vega 18 36 55.4 +38 46 47 HR 2324 HD 45320 06 26 39.6 -01 30 25 HR 2758 HD 56405 07 16 14.6 -15 35 07 HR 4534 HD 102647 11 49 05.2 +14 34 25 HR 8728 HD 216956 22 57 37.7 -29 37 12 HR 553 HD 11636 01 54 38.0 +20 48 34 HR 5062 HD 116842 13 25 12.7 +54 59 18 HR 3662 HD 79439 09 16 11.0 +54 01 16 HR 3321 HD 71297 08 26 27.3 -03 59 12 HR 8270 HD 205924 21 38 31.5 +05 46 16 HR 401 HD 8511 01 24 01.8 -08 00 24 HR 5793 HD 139006 15 34 40.7 +26 42 57 HR 2421 HD 47105 06 37 42.5 +16 24 00 HR 4033 HD 89021 10 17 06.5 +42 54 54 HR 8717 HD 216735 22 55 13.3 +08 48 57 HR 5867 HD 141003 15 46 11.0 +15 25 21 HR 1666 HD 33111 05 07 51.2 -05 05 07 HR 4357 HD 97603 11 14 05.9 +20 31 32 HR 403 HD 8538 01 25 46.9 +60 14 10 HR 622 HD 13161 02 09 31.9 +34 59 16 HR 4294 HD 95382 11 00 44.9 +06 06 06 HR 3569 HD 76644 08 59 14.6 +48 02 41 HR 8518 HD 212061 22 21 38.8 -01 23 15 HR 5291 HD 123299 14 04 23.7 +64 22 32 HR 7950 HD 198001 20 47 40.3 -09 29 43 HR 2751 HD 56169 07 18 31.9 +49 27 53 HR 5735 HD 137422 15 20 43.8 +71 50 01 HR 4189 HD 92769 10 43 02.2 +26 19 35 HD 73210 08 37 46.8 +19 16 03 HR 1412 HD 28319 04 28 39.3 +15 52 16 HR 4555 HD 103313 11 53 50.4 +00 33 07 HR 6095 HD 147547 16 21 55.3 +19 09 09 HR 146 HD 3283 00 36 27.2 +60 19 35 HR 6081 HD 147084 16 20 38.1 -24 10 09 HR 6562 HD 159877 17 37 36.1 -15 34 16 HR 3975 HD 87737 10 07 19.9 +16 45 46 HR 641 HD 13476 02 13 41.5 +58 33 39 HR 6144 HD 148743 16 30 29.8 -07 30 53 HR 1040 HD 21389 03 29 54.8 +58 52 44 HR 7924 HD 197345 20 41 25.8 +45 16 49 HD 164514 18 02 31.6 -22 54 20 HR 1605 HD 31964 05 01 58.1 +43 49 24
Flux data for figure 1, A V stars Lambda Wavelength 0.1nm logF(A0_Va)1 HR 4554 = HD 103287 flux 10mW/m2/nm logF(A0_Va)2 Vega = HD 172167 flux 10mW/m2/nm logF(A1_Va) HR 2324 = HD 45320 flux 10mW/m2/nm logF(A2_Va) HR 2758 = HD 56405 flux 10mW/m2/nm logF(A3_Va)1 HR 4534 = HD 102647 flux 10mW/m2/nm logF(A3_Va)2 HR 8728 = HD 216956 flux 10mW/m2/nm logF(A4_V) HR 553 = HD 11636 flux 10mW/m2/nm logF(A5_Vn) HR 5062 = HD 116842 flux 10mW/m2/nm logF(A6_V) HR 3662 = HD 79439 flux 10mW/m2/nm logF(A7_V) HR 3321 = HD 71297 flux 10mW/m2/nm logF(A8_Vn) HR 8270 = HD 205924 flux 10mW/m2/nm logF(A9_V) HR 401 = HD 8511 flux 10mW/m2/nm Flux data for figure 2, A IV stars Lambda Wavelength 0.1nm logF(A0IV) HR 5793 = HD 139006 flux 10mW/m2/nm logF(A1IVs) HR 2421 = HD 47105 flux 10mW/m2/nm logF(A1IV)1 HR 4033 = HD 89021 flux 10mW/m2/nm logF(A1IV)2 HR 8717 = HD 216735 flux 10mW/m2/nm logF(A2IV) HR 5867 = HD 141003 flux 10mW/m2/nm logF(A3IV) HR 1666 = HD 33111 flux 10mW/m2/nm logF(A4IV) HR 4357 = HD 97603 flux 10mW/m2/nm logF(A5IV)1 HR 403 = HD 8538 flux 10mW/m2/nm logF(A5IV)2 HR 622 = HD 13161 flux 10mW/m2/nm logF(A6IV) HR 4294 = HD 95382 flux 10mW/m2/nm logF(A7IV) HR 3569 = HD 76644 flux 10mW/m2/nm Flux data for figure 3, A III stars Lambda Wavelength 0.1nm logF(B9.5III-IV) HR 8518 = HD 212061 flux 10mW/m2/nm logF(A0III) HR 5291 = HD 123299 flux 10mW/m2/nm logF(A1III-) HR 7950 = HD 198001 flux 10mW/m2/nm logF(A2III) HR 2751 = HD 56169 flux 10mW/m2/nm logF(A3III) HR 5735 = HD 137422 flux 10mW/m2/nm logF(A4III) HR 4189 = HD 92769 flux 10mW/m2/nm logF(A5III) HD 73210 flux 10mW/m2/nm logF(A7III) HR 1412 = HD 28319 flux 10mW/m2/nm logF(A8III) HR 4555 = HD 103313 flux 10mW/m2/nm logF(A9IIIb) HR 6095 = HD 147547 flux 10mW/m2/nm Flux data for figure 4, A II, Ib, Iab stars Lambda Wavelength 0.1nm logF(A3II) HR 146 = HD 3283 flux 10mW/m2/nm logF(A5II) HR 6081 = HD 147084 flux 10mW/m2/nm logF(A7II-) HR 6562 = HD 159877 flux 10mW/m2/nm logF(A0Ib) HR 3975 = HD 87737 flux 10mW/m2/nm logF(A3Iab) HR 641 = HD 13476 flux 10mW/m2/nm logF(A7Ib) HR 6144 = HD 148743 flux 10mW/m2/nm Flux data for figure 5, A Ia stars Lambda Wavelength 0.1nm logF(A0Ia) HR 1040 = HD 21389 flux 10mW/m2/nm logF(A2Ia) HR 7924 = HD 197345 flux 10mW/m2/nm logF(A3Ia) HD 164514 flux 10mW/m2/nm logF(A9Ia) HR 1605 = HD 31964 flux 10mW/m2/nm CDS 1996 Jan 29 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 07-Oct-95 J_ApJ_446_300.xml UIT and optical imagery of Large Magellanic cloud associations LH 52 and LH 53: ages and initial mass function slopes J/ApJ/446/622 J/ApJ/446/622 UV and optical imagery of LH 52 and LH 53 UIT and optical imagery of Large Magellanic cloud associations LH 52 and LH 53: ages and initial mass function slopes R S Hill K -P Cheng R C Bohlin R W OConnell M S Roberts A M Smith T P Stecher Astrophys. J. 446 622 1995 1995ApJ...446..622H Clusters, open Magellanic Clouds Photometry, ultraviolet dust, extinction Magellanic Clouds open clusters and associations: general stars: luminosity function, mass function ultraviolet: stars A 40' field including the stellar associations LH 52 and LH 53 and the supernova remnant N49 in the Large Magellanic Cloud was observed by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Space Shuttle mission in 1990 December. The image in the 162 nm bandpass is discussed together with ground-based BV data on subfields containing LH 52 and LH 53. Point-spread function photometry in the 162nm, B, and V bands is presented in the form of color-magnitude diagrams and two-color diagrams, which are compared with stellar models. The far-ultraviolet extinction curve of the dust in LH 52 is unusually steep for the LMC. The most probable age of both associations is ~10 Myr, which constrains the scenario for the evolution of the supergiant Halpha shell LMC 4 by stochastic self-propagated star formation. The initial mass function (IMF) slope for LH 52 is Gamma~-1, in agreement with previous work, and the slope for LH 53, which is less densely populated, is Gamma~-2. A similar relationship between surface density of stars and IMF slope is reported for a UIT field near 30 Dor. The ultraviolet morphology of N49, which is contained in LH 53, is dominated by two bright features that straddle an X-ray bright spot, consistent with an encounter between the blast wave and a cloud. The estimated age of ~10Myr for LH 53 implies an initial mass of ~20M_{sun}_ for the N49 progenitor star.
ASTRO 1/UIT LH 52 NGC 1948 05 24 -66 24 LH 53 05 26 -66 14
Ultraviolet sources in LH 52 Ultraviolet sources in LH 53 ID Identification IDs are derived from UIT photometry. Duplicates mean the same ultraviolet source had more than one candidate match on the B image, and the author could not decide between them. However, coordinates are based on the B sources and can thus differ between two appearances of the same ID. --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declinatin sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec m162 Magnitude at 162nm m162 = -2.5*alog10(f_B5) - 21.1, where f_B5 is the mean flux in the UIT B5 bandpass in mW/m2/(0.1nm); the B5 centroid wavelength is approximately 162nm. mag e_m162 DAOPHOT-type internal error in m162 mag Bmag Calibrated B magnitude mag e_Bmag DAOPHOT-type internal error in Bmag mag Vmag Calibrated V magnitude mag e_Vmag DAOPHOT-type internal error in V mag Remark Remark on dup. matches or UIT image quality --- BV photometry of LH 52 BV photometry of LH 53 ID Identification derived from V photometry --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Bmag B magnitude mag e_Bmag DAOPHOT-like internal error mag Vmag V magnitude mag e_Vmag DAOPHOT-like internal error mag CDS 1996 Jan 29 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 10-Oct-95 J_ApJ_446_622.xml The intermediate stellar mass population in R136 determined from Hubble Space Telescope planetary camera 2 images J/ApJ/448/179 J/ApJ/448/179 HST photometry in R136 The intermediate stellar mass population in R136 determined from Hubble Space Telescope planetary camera 2 images D A Hunter E J Shaya J A Holtzman R M Light E J Oneil Jr. R Lynds Astrophys. J. 448 179 1995 1995ApJ...448..179H Clusters, open Magellanic Clouds Photometry Hertzsprung-Russell (HR diagram) Magellanic Clouds open clusters and associations: individual (R136) stars: evolution stars: luminosity function, mass function We have analyzed Hubble Space Telescope (HST) images of the compact, luminous star cluster R136 in the LMC that were taken with the refurbished HST and new Wide Field/Planetary Camera. These images allow us to examine the stellar population in a region of unusually intense star formation at a scale of 0.01pc. We have detected stars to 23.5 in F555W and have quantified the stellar population to an M_555.0 of 0.9 or a mass of 2.8M_{sun}_. Comparisons of HR diagrams with isochrones that were constructed for the HST flight filter system from theoretical stellar evolutionary tracks reveal massive stars, a main sequence to at least 2.8M_{sun}_, and stars with M_555.0>=0.5 still on pre-main sequence tracks. The average stellar population is fit with a 3-4Myr isochrone. Contrary to expectations from star formation models, however, the formation period for the massive stars and lower mass stars appear to largely overlap. We have measured the IMF for stars 2.8-15M_{sun}_ in three annuli from 0.5-4.7pc from the center of the cluster. The slopes of the IMF in all three annuli are the same within the uncertainties, thus, showing no evidence for mass segregation beyond 0.5pc. Furthermore, the combined IMF slope, -1.22+/-0.06, is close to a normal Salpeter IMF. The lower mass limit must be lower than the limits of our measurements: <=2.8M_{sun}_ beyond 0.5pc and <=7M_{sun}_ within 0.1pc. This is contrary to some predictions that the lower mass limit could be as high as 10M_{sun}_ in regions of intense massive star formation. Integrated properties of R136 are consistent with its being comparable to a rather small globular cluster when such clusters were the same age as R136. From the surface brightness profile, an upper limit for core radius of 0.02pc is set. Within a radius of 0.4pc we estimate that there have been roughly 20 crossing times and relaxation should be well along. Within 0.5pc crowding prevents us from detecting the intermediate mass population, but there is a hint of an excess of stars brighter than M_555.0=-5 and of a deficit in the highest mass stars between 0.6pc and 1.2pc. This would be consistent with dynamical segregation.
R 136 RMC 136 HD 38268 05 38 42.8 -69 06 03
The photometry Star Star identification number --- Xpos X pixel coordinate The X,Y coordinates are those in the short exposure F555W image, and the coordinate system is indicated in Figure 2 of the printed paper. pix Ypos Y pixel coordinate pix F336W F336W magnitude mag e_F336W F336W magnitude uncertainty mag F555W F555W magnitude mag e_F555W F555W magnitude uncertainty mag F814W F814W magnitude mag e_F814W F814W magnitude uncertainty mag F336W-F555W F336W-F555W color mag e_F336W-F555W F336W-F555W color uncertainty mag F555W-F814W F555W-F814W color mag e_F555W-F814W F555W-F814W color uncertainty mag CDS 1996 Jan 29 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 10-Oct-95 J_ApJ_448_179.xml ROSAT all-sky survey observations of the Hyades cluster J/ApJ/448/683 J/ApJ/448/683 Hyades RASS observations ROSAT all-sky survey observations of the Hyades cluster R A Stern J H M M Schmitt P T Kahabka Astrophys. J. 448 683 1995 1995ApJ...448..683S IX/11 : The ROSAT Source Catalogue (Voges+ 1995) Binaries, X-ray Clusters, open binaries: close open clusters and associations: individual (Hyades) surveys X-rays: stars We report the results of a complete X-ray survey of the Hyades cluster region using the ROSAT All-Sky Survey (RASS). Our survey covers over 900deg^2^ of the sky. Over 185 optically identified Hyades were detected down to a limiting X-ray luminosity of ~1-2x10^28^ergs/s (0.1-1.8keV); among solar-like stars, i.e., main-sequence stars of spectral type G, the RASS detection rate is ~90%. The presence of many binary systems in the cluster is a key factor influencing the X-ray luminosity function. Short-period (~ a few days or less) binaries are anomalously X-ray bright, as might be expected; however, the X-ray luminosity functions of K and possibly M binaries of all types are significantly different from their single counterparts, confirming the results of Pye et al. (1994MNRAS.266..798P) for a smaller K star sample drawn from deep ROSAT pointings. Comparison with Einstein Observatory studies of a subset of Hyades stars demonstrates a general lack of significant (> a factor of 2) long-term X-ray variability. This may be the result of the dominance of a small-scale, turbulent dynamo in the younger Hyades stars compared to the large-scale, cyclic dynamo observed in the Sun.
ROSAT
Hyades survey Star Star name number=1 For members with multiple designations, the name used is determined by the following order of preference: vB (van Bueren, 1952BAN....11..385V), VA (van Altena, 1969AJ.....74....2V), BD (Bonner Durchmusterung, Cat. <I/122>), GH 7 or GH 8 (Giclas, Burnham, & Thomas, 1962LowOB...5..257G), L (Pels et al., 1975A&A....43..423P), LP (Luyten et al., 1981, see Cat. <I/130>), H (Hanson 1975, Cat. <J/AJ/80/379>), OS (Osvald, 1954AN....281..193O), AK (Artyukhina & Khopolov 1975, Trans. Gos. Astron. Inst. Sternberg, 46 No. 2, 57 and 1976, Trans. Gos. Astron. Inst. Sternberg, 47 ,105) HD, or other designation. A table of cross-referenced Hyades members provided by E. Weis was used in selecting the primary designation. --- RAh Optical right ascension (J2000) h RAm Optical right ascension (J2000) min RAs Optical right ascension (J2000) s DEd Optical declination (J2000) deg DEm Optical declination (J2000) arcmin DEs Optical declination (J2000) arcsec X-Opos Difference in X-ray and optical positions arcsec Vmag V magnitude mag r_Vmag Reference for V magnitude number=2 Optical photometry references are as follows: (1)-(3) Weis & Hanson, 1988AJ.....96..148W (4)-(6) Upgren et al., 1985AJ.....90.2039U (7) Weis, 1983PASP...95...29W (8)-(9) Weis & Upgren, 1982PASP...94..475W (10) Stauffer, 1982AJ.....87..899S (11) Weis et al., 1979PASP...91..766W (12)-(13) Weis, 1992, unpublished photometry; (14) Pels et al., 1975A&A....43..423P (15) Eggen, 1969ApJ...157..287E (16) Morel & Mangnenat, 1978, Cat. <II/7> (17) Schwan, 1991A&A...243..386 (18) Reid, 1992, Cat. <J/MNRAS/257/257> (19) Hanson, 1975, Cat. <J/AJ/80/379> (20) Griffin et al., 1988AJ.....96..172G --- B-V B-V colour index mag r_B-V Reference for B-V index number=2 Optical photometry references are as follows: (1)-(3) Weis & Hanson, 1988AJ.....96..148W (4)-(6) Upgren et al., 1985AJ.....90.2039U (7) Weis, 1983PASP...95...29W (8)-(9) Weis & Upgren, 1982PASP...94..475W (10) Stauffer, 1982AJ.....87..899S (11) Weis et al., 1979PASP...91..766W (12)-(13) Weis, 1992, unpublished photometry; (14) Pels et al., 1975A&A....43..423P (15) Eggen, 1969ApJ...157..287E (16) Morel & Mangnenat, 1978, Cat. <II/7> (17) Schwan, 1991A&A...243..386 (18) Reid, 1992, Cat. <J/MNRAS/257/257> (19) Hanson, 1975, Cat. <J/AJ/80/379> (20) Griffin et al., 1988AJ.....96..172G --- Dist Distance pc r_Dist Reference for distance number=3 H: Hanson, 1975, Cat. <J/AJ/80/379> S: Schwan, 1991A&A...243..386 --- Binarity Binarity codes number=4 Binary notations: GR: spectroscopic binary as noted in Griffin et al., 1988AJ.....96..172G GP: photometric binary as noted in Griffin et al., 1988AJ.....96..172G GV: visual binary as noted in Griffin et al., 1988AJ.....96..172G B: spectroscopic binary listed in Batten et al., 1989, Cat. <V/64> C: photometric binary from Carney, 1982AJ.....87.1527C T: photometric binary as noted by Bettis, 1975 (reference not precised) S: photometric binary as noted by Stauffer, 1982AJ.....87..899S UW: photometric binary as noted by Upgren & Weis, 1977AJ.....82..978U A: visual binary in ADS catalog MD: definite speckle binary in Mason et al., 1993AJ....105..220M MP: probable speckle binary in Mason et al., 1993AJ....105..220M MS: suspected speckle binary in Mason et al., 1993AJ....105..220M SP: spectroscopic binary or triple based on unpublished data (Stauffer, private communication). --- M/L Maximum likelihood ratio for X-ray source existence --- l_LX45 Limit flag on LX45 --- LX45 X-ray luminosity based upon an assumed 45pc distance ZW e_LX45 rms uncertainty on LX45 ZW l_LXd Limt flag on LXd --- LXd X-ray luminosity using the distance from Dist column ZW e_LXd rms uncertainty on LXd ZW Reid (1992, Cat. <J/MNRAS/257/257>) stars detected in X-rays Star Star designation (Reid number, Cat. <J/MNRAS/257/257>) --- RAh Optical right ascension (J2000) h RAm Optical right ascension (J2000) min RAs Optical right ascension (J2000) s DEd Optical declination (J2000) deg DEm Optical declination (J2000) arcmin DEs Optical declination (J2000) arcsec Vmag V magnitude mag B-V B-V colour index mag M/L Maximum likelihood ratio for X-ray source existence --- PSPC PSPC count ct/s e_PSPC rms uncertainty on PSPC ct/s X-Opos Difference in X-ray and optical positions arcsec Note Notes --- Non-members in optical catalog detected in X-rays Star Star name --- RAh Optical right ascension (J2000) h RAm Optical right ascension (J2000) min RAs Optical right ascension (J2000) s DEd Optical declination (J2000) deg DEm Optical declination (J2000) arcmin DEs Optical declination (J2000) arcsec Vmag V magnitude mag B-V B-V colour index mag Binarity Binarity codes number=1 Binary notations: GR: spectroscopic binary as noted in Griffin et al., 1988AJ.....96..172G UW: photometric binary as noted by Upgren & Weis, 1977AJ.....82..978U --- M/L Maximum likelihood ratio for X-ray source existence --- PSPC PSPC count ct/s e_PSPC rms uncertainty on PSPC ct/s X-Opos Difference in X-ray and optical positions arcsec James Marcout, Patricia Bauer CDS 1997 Apr 08 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_448_683.xml Variable Stars in Magellanic Cloud Clusters. II. NGC 1850 J/ApJ/449/164 J/ApJ/449/164 Variable Stars in MC Clusters. II Variable Stars in Magellanic Cloud Clusters. II. NGC 1850 P R Sebo K M Wood Astrophys. J. 449 164 1995 1995ApJ...449..164S Clusters, open Magellanic Clouds Photometry, CCD Stars, variable Cepheids Magellanic Clouds open clusters and associations: general stars: evolution In the case where there are differing numbers of data points in each color, the color with the fewer data points has been padded with zeros. We present the results of a study aimed at identifying variable stars in the rich LMC cluster NGC 1850. V and I band CCD imaging spanning more than 5 years in a 10'x10' field surrounding the cluster has allowed us to identify more than 30 variable stars, including seven classical Cepheids, one anomalous Cepheid, two RR Lyrae variables, 19 long-period variables (LPVs), one blue eclipsing binary, one possible pair of eclipsing giants, and several peculiar variables. The only likely cluster member is a Cepheid. Isochrone fitting to the cluster CMD yields an age of 80 Myr if an LMC distance modulus of 18.5 is adopted. A comparison of pulsation and evolution masses for the Cepheids still yields a ratio of evolution to pulsation mass of ~1.2 for evolution models computed with core overshoot parameter Lambda = 0.5, where Lambda = 2d_ov/H_p, d_ov is the distance that convection overshoots beyond the Schwarzschild boundary and H_p is the pressure scale height. An overshoot parameter Lambda ~ 1.0 would be required to bring the evolution and pulsation masses into agreement. One of the Cepheids in the field is a bump Cepheid. A calculation of the bump mass yields a value in reasonable agreement with the pulsation mass. We show that detailed modelling of individual bump Cepheids is capable of providing very tight constraints on the LMC distance modulus. The Cepheid period-luminosity-color relation compared to the theoretical relation yields a LMC distance modulus of 18.60. Finally, arguments are presented which suggest that the LPVs are a mixture of fundamental mode pulsators and small-amplitude overtone pulsators.
NGC 1850 SW 9 05 08 18.4 -68 46 46 NGC 1850 SW 17 05 08 44.1 -68 45 28 NGC 1850 SW 39 05 08 28.2 -68 48 24 NGC 1850 SW 58 05 08 43.6 -68 45 33 NGC 1850 SW 110 05 09 16.0 -68 44 30 NGC 1850 SW 120 05 09 24.3 -68 47 24 NGC 1850 SW 269 05 08 54.9 -68 43 10 NGC 1850 SW 341 05 08 07.3 -68 41 09 NGC 1850 SW 347 05 08 12.9 -68 41 03 NGC 1850 SW 349 05 08 16.4 -68 48 38 NGC 1850 SW 395 05 08 39.6 -68 43 46 NGC 1850 SW 441 05 09 08.8 -68 48 53 NGC 1850 SW 502 05 09 35.8 -68 41 43 NGC 1850 SW 504 05 09 38.4 -68 48 07 NGC 1850 SW 558 05 08 05.0 -68 42 12 NGC 1850 SW 574 05 08 09.4 -68 43 22 NGC 1850 SW 587 05 08 14.5 -68 44 55 NGC 1850 SW 652 05 08 28.3 -68 45 04 NGC 1850 SW 670 05 08 32.5 -68 44 30 NGC 1850 SW 679 05 08 35.4 -68 48 59 NGC 1850 SW 1038 05 09 28.3 -68 47 51 NGC 1850 SW 1078 05 09 41.6 -68 45 26 NGC 1850 SW 1084 05 09 42.5 -68 45 16 NGC 1850 SW 1135 05 08 14.3 -68 49 42 NGC 1850 SW 1847 05 09 00.5 -68 47 02 NGC 1850 SW 1906 05 09 05.6 -68 46 30 NGC 1850 SW 1956 05 09 10.1 -68 41 38 NGC 1850 SW 2093 05 09 20.5 -68 45 54 NGC 1850 SW 2199 05 09 31.8 -68 48 52 NGC 1850 SW 2202 05 09 30.5 -68 42 27 NGC 1850 SW 2268 05 09 39.7 -68 45 35 NGC 1850 SW 9276 05 09 47.9 -68 45 08 NGC 1850 SW 10753 05 08 19.6 -68 44 44
V photometry Star Number of star --- JD Julian date of V observation d Vmag V magnitude mag e_Vmag V magnitude error mag I photometry Star Number of star --- JD Julian date of I observation d Imag I magnitude mag e_Imag I magnitude error mag CDS 1996 Jan 29 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 10-Oct-95 UNKNOWN UNKNOWN The original 34 files were merged into two files J_ApJ_449_164.xml Large-scale structures in the zone of avoidance: the galactic anticenter region J/ApJ/449/527 J/ApJ/449/527 Galaxies in the zone of avoidance Large-scale structures in the zone of avoidance: the galactic anticenter region N Y Lu W Freudling Astrophys. J. 449 527 1995 1995ApJ...449..527L II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) Galaxies, IR Infrared sources galaxies: clusters: general galaxies: distances and redshifts radio lines: galaxies We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h<RA<10h and 0deg<DE<36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA<3h from structures at RA>4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully & Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.
IRAS
List of the candidate sources IRAS IRAS name --- m_IRAS Multiplicity index on IRAS --- n_IRAS Note on IRAS number=1 An * indicates PSC sources which fail to pass our selection criteria. --- GLAT Galactic latitude deg n1 Object category number=2 1: Catalogued galaxies, i.e., sources flagged in the PSC to be associated with one or more optical galaxy catalogs 2: Galactic sources (as marked in the PSC) 3: pure IRAS source --- n2 Observed in one 21 cm H I survey number=3 A nonzero number indicates that the source was observed in one of the two similar 21cm HI surveys over a velocity coverage of (0-8000)km/s, where 1=the current survey and 2=Lu et al. (1990ApJ...357..388L) --- n3 Observed in one 21 cm H I survey number=4 An index of unity means that the source was observed in the current survey over a velocity coverage of (8000-16000)km/s --- HV Heliocentric velocity km/s Ref References number=5 Reference that gives either the original redshift or identification, or the original work of the redshift or identification. 1: this paper 2: Lu et al. (1990ApJ...357..388L) 3: Pantoja et al. (1994AJ....108..921P) 4: Giovanelli & Haynes (1993, Cat. <J/AJ/105/1271>) 5: the Third References Catalogue of Galaxies, de Vaucouleurs et al., 1991, Cat. <VII/155> 6: the NASA/IPAC Extragalactic Database (Helou et al., 1991, in Database and On-Line Data in Astronomy, ed. M.A. Albrecht & D. Egret (Dordrecht: Kluwer), 89) 7: Strauss et al. (1992, Cat. <II/174>) 8: IRAS-1,2Jy redshift catalog (Strauss 1994 (Priv. Comm.), see also Fisher et al. 1992ApJ...389..188F) 9: the 1-in-6 redshift catalog of the Queen Mary-West Field College, Durham, Oxford, and Toronto (Lawrence et al. 1994, preprint) 10: Takata et al. (1994, Cat. <J/A+AS/104/529>) 11: the catalog of IRAS point source redshift survey (Saunders 1994 (Priv. Comm.), see also Rowan-Robinson et al. (1991MNRAS.253..485R) --- H I 21cm data of the detected galaxies IRAS IRAS name --- m_IRAS Multiplicity index on IRAS --- HV50 Mean heliocentric velocity, taken to be the middle point between the velocities at the flux level 50% of the peak(s) on either side of the profile km/s l_Wm20 Limit flag on Wm20 --- Wm20 Velocity width at 20% of the mean flux density within the profile km/s l_Wm50 Limit flag on Wm50 --- Wm50 Velocity width at 50% of the mean flux density within the profile km/s Wp20 Velocity width at 20% of the peak(s) km/s Wp50 Velocity width at 50% of the peak(s) km/s Wp80 Velocity width at 80% of the peak(s) km/s SHI Integrated HI flux Jy.km/s S/N Observed ratio of peak signal-to-noise --- Notes Notes number=1 1: Widths are ambiguous 2: The galaxy was detected in the OFF spectrum taken at the same declination as the ON position but at an R.A. that is 117.0' east of the ON position 3: The peak widths are probably incorrect 4: Possibly two galaxies along the line of sight 5: The high-velocity wing of the profile is slightly beyond our limiting velocity 6: The galaxy was detected in the OFF spectrum taken at the same declination as the ON position, but at an R.A. that is 91.8' east of the ON position 7: The galaxy was detected in the OFF spectrum taken at the same declination as the ON position, but at an R.A. that is 109.5' east of the ON position --- James Marcout, Patricia Bauer CDS 1997 Apr 01 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_449_527.xml Triggered star formation and the dynamics of a superbubble in the LMC: the OB association LH 47/48 in DEM 152 J/ApJ/452/210 J/ApJ/452/210 UBV photometry in LH 47/48 Triggered star formation and the dynamics of a superbubble in the LMC: the OB association LH 47/48 in DEM 152 M S Oey P Massey Astrophys. J. 452 210 1995 1995ApJ...452..210O Associations, stellar Magellanic Clouds Photometry, UBV galaxies: star clusters ISM: bubbles ISM: individual (DEM 152) Magellanic Clouds stars: formation We examine the stellar population of an OB association, LH 47/48, which is associated with a superbubble H II region, DEM 152 in the N44 nebular complex of the Large Magellanic Cloud. With CCD photometry and spectroscopy of the massive stars, we find no evidence that an unusual stellar population gave rise to the shell morphology of the gas. The slope of the initial mass function, {GAMMA}=1.3+/-0.2, is consistent with that of other OB associations in the LMC, and there is no significant difference in the initial mass function internal or external to the supershell. The inferred stellar ionizing flux is consistent with the observed nebular H alpha flux. We do find evidence for triggered star formation: the H-R diagram suggests an age of >10Myr for the population interior to the bubble with more recent, <5Myr, star formation on the exterior. Using the detailed data on the stellar population, we compare a numerical form of the Weaver et al. (1977ApJ...218..377W) evolutionary model for wind-driven bubbles with the observed shell kinematics. We find a substantial discrepancy: the observed shell radius is too small and/or expansion velocity too large to be explained with this version of the model. We discuss possible explanations for the inconsistency.
LH 47 HD 35814 NGC 1935 05 22.0 -67 57 LH 48 NGC 1937 05 22.5 -67 53
Photometry of stars in LH 47 photometry of stars in LH 48 Star Star number --- m_Star Multiuplicity index on Star --- Xpos X position pix Ypos Y position pix Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag Derived parameter stars with spectral types Star Star designation --- Xpos X position pix Ypos Y position pix RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag Q Reddening-free parameter (Q=(U-B)-0.72(B-V)) --- log(Teff) Effective temperature K u_log(Teff) Uncertainty flag on log(Teff) --- Mbol Bolometric magnitude mag u_Mbol Uncertainty flag on Mbol --- Mass Star mass solMass u_Mass Uncertainty flag on Mass --- SpType Spectral type --- James Marcout, Patricia Bauer CDS 1997 Apr 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_452_210.xml The Massive Stars of I Zw 18 as Seen in Hubble Space Telescope Images J/ApJ/452/238 J/ApJ/452/238 HST photometry of I Zw 18 massive stars The Massive Stars of I Zw 18 as Seen in Hubble Space Telescope Images D A Hunter H A Thronson Astrophys. J. 452 238 1995 1995ApJ...452..238H Photometry Stars, early-type galaxies: compact galaxies: individual (I Zw 18) galaxies: stellar content stars: early-type Blue compact dwarf galaxies are tiny galaxies that are dominated by intense star-forming regions. Thus, they have been thought to represent a different and extreme environment for star formation compared to the Milky Way and many other nearby galaxies. In this paper we use images obtained with the Hubble Space Telescope to resolve the main body of one of these galaxies, I Zw 18, into stars for the first time. This galaxy is also one of the most metal-poor galaxies known and is sometimes argued to be evolutionarily young. Broadband colors are used to determine the bulk characteristics of the resolved stellar population to an F555W magnitude of about 26, or M_(V,0)~-4 (O9.5 V star). Narrow-band images are used to look for emission characteristic of Wolf-Rayet stars. Color-magnitude diagrams reveal a broad main sequence of massive stars as well as blue and red supergiants, although there is a surprising lack of Wolf-Rayet stars. About half the massive stars are located in two groups, corresponding to the two knots of emission identified in ground-based images, and the rest are distributed between these regions and in the outer parts of the galaxy. We find that the northwestern of these two regions resolves in Halpha images into a small H II region plus a complicated shell structure that encircles the northern stellar association. There are additional, larger loops and filaments of ionized gas up to 450pc from the center of the galaxy. While the shell could be as young as the stars it encircles, the larger ionized gas structures must be older for reasonable models, and their presence implies that there has been a previous generation of massive stars at least several tens of millions of years ago. However, we find no evidence in these data for stars that must be older than this. The larger sites of most recent star formation are located northwest and south of the central part of the galaxy. Thus, we find that I Zw 18 is somewhat more complicated than had previously been thought, both in terms of its star formation history and the state of its interstellar medium. At the same time, however, the stellar populations look relatively normal, and the spatial concentration of massive stars is closer to that of large OB associations in nearby galaxies rather than to that exemplified by the compact cluster R136 in the Large Magellanic Cloud.
I Zw 18 Mkn 116 Mrk 116 ZW I 18 09 34 02.1 +55 14 25
The photometry Star Star identification number --- Xpos X pixel coordinate The X,Y coordinates are those in the F555W image, and the coordinate system is indicated in Figure 2 of the printed paper. pix Ypos Y pixel coordinate pix F336W F336W magnitude mag e_F336W F336W magnitude uncertainty mag F555W F555W magnitude mag e_F555W F555W magnitude uncertainty mag F814W F814W magnitude mag e_F814W F814W magnitude uncertainty mag F336W-F555W F336W-F555W color mag e_F336W-F555W F336W-F555W color uncertainty mag F555W-F814W F555W-F814W color mag e_F555W-F814W F555W-F814W color uncertainty mag UNKNOWN 1996 Jan 29 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 11-Oct-95 J_ApJ_452_238.xml The contribution of late-type/irregulars to the faint galaxy counts from Hubble Space Telescope Medium Deep Survey images J/ApJ/453/48 J/ApJ/453/48 VI photometry of HST faint field galaxies The contribution of late-type/irregulars to the faint galaxy counts from Hubble Space Telescope Medium Deep Survey images S P Driver R A Windhorst R E Griffiths Astrophys. J. 453 48 1995 1995ApJ...453...48D Galaxies, photometry Morphology galaxies: evolution galaxies: fundamental parameters galaxies: irregular galaxies: luminosity function, mass function galaxies: starburst surveys We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=<Imag<22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)<1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M & 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z>=0.5 at m_I_=21.75mag.
HST
A complete catalog of HST field galaxies obtained from the six MDS fields ID Object identification number --- MDS MDS field name --- WFPC2 WFPC2 CCD number (1=PC, 2, 3, 4=WFC) --- Xpos Original X pixel position on the WFPC2 CCD pix Ypos Original Y pixel position on the WFPC2 CCD pix RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) number=1 Relative RAs and DEs should be accurate to within 0.1". Absolute WFPC2 astrometry is only accurate to ~0.5"-1." s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) number=1 Relative RAs and DEs should be accurate to within 0.1". Absolute WFPC2 astrometry is only accurate to ~0.5"-1." arcsec Imag Total I_814_ magnitude mag V-I Total (V-I) color mag SuBr Central I-band surface brightness within a radius of 0.2" mag/arcsec2 (V-I)c Central (V-I) color within a radius of 0.2" mag eps Image ellipticity e=1-a/b, computed from the outermost isophote --- Mtype Galaxy type number=2 0 = E, 1 = 5a, 2 = 5b, 3 = 5c, 4 = 5d, 5 = Irr, 6 = peculiar --- Radius Aperture radius used to determine the I-band magnitude pix James Marcout, Patricia Bauer CDS 1997 Feb 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_453_48.xml Multiwavelength energy distributions and bolometric luminosities of the 12 micron galaxy sample J/ApJ/453/616 J/ApJ/453/616 JHKL photometry of 12 micron galaxy sample Multiwavelength energy distributions and bolometric luminosities of the 12 micron galaxy sample L Spinoglio M A Malkan B Rush L Carrasco E Recillas-Cruz Astrophys. J. 453 616 1995 1995ApJ...453..616S VII/157 : The extended 12um galaxy sample (Rush+ 1993) Galaxies, photometry Photometry, infrared galaxies: active galaxies: nuclei galaxies: photometry galaxies: Seyfert galaxies: starburst infrared: galaxies Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.
</tableLink> <tableLink xlink:href="table2"> <title>Near-IR photometry of galaxies excluded from the 12 micron sample Name Name of galaxy --- RAh Right ascension (B1950.0), from IRAS FSC Positions from IRAS FSC <II/156>. Blank when the galaxy is not in IRAS FSC. h RAm Right ascension (B1950.0), from IRAS FSC min RAs Right ascension (B1950.0), from IRAS FSC s DE- Declination sign --- DEd Declination (B1950.0), from IRAS FSC deg DEm Declination (B1950.0), from IRAS FSC arcmin DEs Declination (B1950.0), from IRAS FSC arcsec FnuJ J-band flux density mJy u_FnuJ FnuJ uncertainty flag --- FnuH H-band flux density mJy u_FnuH FnuH uncertainty flag --- FnuK K-band flux density mJy u_FnuK FnuK uncertainty flag --- FnuL L-band flux density mJy u_FnuL FnuL uncertainty flag --- Diam Diameter of observing aperture arcsec Date Site (ESO or SPM [San Pedro Martir]) and date --- Type Object Type: 1, 2 = Seyfert1,2; 3 = IR-luminous; 4 = Liner; 0 = normal --- Flag Flags explaining why object was observed a: originally in the 12-Micron Sample, based on its flux in the FSC-2, but later excluded because the ADDSCAN flux is below the sample limit (see Appendix A of Rush, Malkan, and Spinoglio 1993 <VII/157>, hereafter RMS93) b: in Spinoglio & Malkan (1989ApJ...342...83S) c: unidentified object excluded from the 12-Micron Sample in RMS93 <VII/157> (see Table 12 of RMS93). --- Derived NIR parameters for the 12 micron galaxy sample Name Name of galaxy --- z Redshift (corrected as described in RMS93) --- log(FJmag) Computed total flux in the J band mJy log(FHmag) Computed total flux in the H band mJy log(FKmag) Computed total flux in the K band mJy J-H J-H color, smallest available aperture mag H-K H-K color, smallest available aperture mag K-L K-L color, smallest available aperture mag Apert Aperture for colors (for [H-K] if different for each) arcsec log(LNIR) Luminosity integrated over 1.2-3.4um 10-7W log(LFIR) Luminosity integrated over IRAS wavebands 10-7W log(LTOT) Bolometric luminosity 10-7W Type Object Type: 1, 2 = Seyfert1,2; 3 = IR-luminous; 4 = Liner; 0 = normal --- Flag Flags pertaining to apertures and colors a A Seyfert galaxy for which the authors only have whole-galaxy (extrapolated) colors and thus no aperture is given b An object for which no aperture was given with the reference, but where the authors can assume that these are whole-galaxy fluxes because it is very point-like J The [J-H] is from a larger aperture than the [H-K] color (10 objects) L The [K-L] is from a larger aperture than the [H-K] color (7 objects) --- CDS 1996 Jan 29 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 04-Nov-95 J_ApJ_453_616.xml The Initial Mass Function and Massive Star Evolution in the OB Associations of the Northern Milky Way J/ApJ/454/151 J/ApJ/454/151 OB Associations of the Northern Milky Way The Initial Mass Function and Massive Star Evolution in the OB Associations of the Northern Milky Way P Massey K E Johnson K De Gioia-Eastwood Astrophys. J. 454 151 1995 1995ApJ...454..151M Associations, stellar Photometry, UBV Stars, early-type open clusters and associations: general stars: early-type stars: evolution stars: luminosity function, mass function stars: Wolf-Rayet We investigate the massive star content of Milky Way clusters and OB associations in order to answer three questions: (1) How coeval is star formation? (2) How constant is the initial mass function (IMF)? (3) What is the progenitor mass of Wolf-Rayet stars? Our sample includes NGC 6823/Vul OB1, NGC 6871/Cyg OB3, Berkeley 86/Cyg OB1, NGC 6913/Cyg OB1, NGC 7235, NGC 7380/Cep OB1, Cep OB5, IC 1805/Cas OB6, NGC 1893/Aur OB2, and NGC 2244/Mon OB2. Large-field CCD imaging and multiobject, fiber spectroscopy has resulted in UBV photometry for >10,000 stars and new spectral types for ~200 stars. These data are used to redetermine distances and reddenings for these regions and to help exclude probable nonmembers in constructing the H-R diagrams. We reanalyze comparable data previously published on Cyg OB2, Tr 14/16, and NGC 6611 and use all of these to paint a picture of star formation and to measure the IMFs. We find the following: (1) Most of the massive stars are born during a period Delta(Tau) < 3 Myr in each association. Some star formation has clearly preceded this event, as evidenced by the occasional presence of evolved (Tau ~ 10 Myr) 15 Msun stars despite a typical age Tau ~ 2 Myr for the more massive population. However, all these regions also show evidence of 5-10 Msun pre-main-sequence stars (Tau < 1 Myr), demonstrating that some star formation at lower masses does continue for at least 1 Myr after the formation of high-mass stars. (2) There is no statistically significant difference in IMF slopes among these clusters, and the average value is found to be Gamma = -1.1 +/- 0.1 for stars with masses > 7 Msun. A comparison with similarly studied OB associations in the Magellanic Clouds reveals no difference in IMF slope, and hence we conclude that star formation of massive stars in clusters proceeds independently of metallicity, at least between z = 0.02 and z = 0.002. The masses of the highest mass stars are approximately equal in the Milky Way, LMC, and SMC associations, contrary to the expectation that this value should vary by a factor of 3 over this metallicity range. We conclude that radiation pressure on grains must not limit the mass of the highest mass star that can form, in accord with the suggestion of Wolfire & Cassinelli that the mere existence of massive stars suggests that shocks or other mechanisms have disrupted grains in star-forming events. (3) The four Wolf-Rayet stars in our sample have come from stars more massive than 40 Msun; one WC star and one late-type WN star each appear to have come from very massive (~100 Msun) progenitors.
</tableLink> <tableLink xlink:href="cep_ob5.dat"> <title>Catalog data for Cep OB5 Catalog data for IC 1805/Cas OB6 Catalog data for NGC 1893/Aur OB2 Catalog data for NGC 2244/Mon OB2 Catalog data for NGC 6823/Vul OB1 Catalog data for NGC 6871/Cyg OB3 Catalog data for NGC 6913/Cyg OB1 Catalog data for NGC 7235 Catalog data for NGC 7380/Cep OB1 RAh Right ascension, 2000 h RAm R.A. min RAs R.A. s DE- Declination sign --- DEd Declination, 2000 deg DEm Dec. arcmin DEs Dec. arcsec Vmag V magnitude mag u_Vmag V uncertainty flag --- B-V B-V color number=1 These 2 columns (B-V and U-B) are inverted on the AAS CD-ROM mag u_B-V B-V uncertainty flag --- U-B U-B color number=1 These 2 columns (B-V and U-B) are inverted on the AAS CD-ROM mag u_U-B U-B uncertainty flag --- SpNew Newly determined spectral type, if any --- ID Other identification, if any --- SpLit Spectral type from the literature, if any --- CDS 1996 Nov 13 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 05-Nov-95 UNKNOWN UNKNOWN * 08-Nov-1996: the file names corresponding to Berkeley 86 and NGC 6913 have been corrected (see Note(1) in File Summary above) * 18-Nov-1996: column names B-V/U-B inverted in the Byte-by-byte description (see Note(1) in Byte-by-byte description) J_ApJ_454_151.xml Dynamics of the Galactic globular cluster NGC 3201 J/ApJ/454/788 J/ApJ/454/788 Radial velocities and BV photometry of NGC 3201 Dynamics of the Galactic globular cluster NGC 3201 P Cote D L Welch P Fischer K Gebhardt Astrophys. J. 454 788 1995 1995ApJ...454..788C Clusters, globular Photometry, CCD Radial velocities globular clusters: individual (NGC 3201) stars: kinematics techniques: radial velocities BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5<~R<~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.
Radial velocities and photometry Star Star identification number --- RAh Right ascension, equinox=2000.0 h RAm Right ascension min RAs Right ascension s DE- Declination sign --- DEd Declination, equinox=2000.0 deg DEm Declination arcmin DEs Declination arcsec Dist Distance from cluster center arcmin HJD HJD of radial velocity d HRV Heliocentric radial velocity km/s e_HRV HRV uncertainty km/s HRVmean Weighted mean heliocentric radial velocity km/s e_HRVmean HRVmean uncertainty km/s Vmag Apparent V magnitude mag B-V Apparent B-V color mag o_HRV Number of radial velocity measurements --- Chi2 Chi-square for radial velocities --- Chi2_R Reduced chi-square for radial velocities --- Prob Probability of obtaining a chi-square this large purely as a consequence of measurement error --- Src Source of photometry, 'APM' or 'CCD' --- Patricia Bauer CDS 1996 Oct 24 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 05-Nov-95 J_ApJ_454_788.xml The Canada-France Redshift Survey: II. Spectroscopic program : data for the 0000-00 and 1000+25 fields J/ApJ/455/60 J/ApJ/455/60 CFRS II: 0000-00 and 1000+25 fields The Canada-France Redshift Survey: II. Spectroscopic program : data for the 0000-00 and 1000+25 fields O Le Fevre D Crampton S J Lilly F Hammer L Tresse Astrophys. J. 455 60 1995 1995ApJ...455...60L J/ApJ/455/75 : CFRS III: 1415+52 and 2215+00 fields (Lilly+ 1995) J/ApJ/455/88 : CFRS IV: 0300+00 field (Hammer+ 1995) J/ApJ/464/79 : CFRS XI: High-redshift field galaxies morphology (Schade+ 1996) Lilly S.J. et al., Paper I. =1995ApJ...455...50L Lilly S.J. et al., Paper III. =1995ApJ...455...75L, Cat. <J/ApJ/455/75> Hammer F. et al., Paper IV. =1995ApJ...455...88H, Cat. <J/ApJ/455/88> Crampton D. et al., Paper V. =1995ApJ...455...96C Lilly S. J. et al., Paper VI. =1995ApJ...455..108L Hammer F. et al., Paper VII. =1995MNRAS.276.1085H Le Fevre O. et al., Paper VIII. =1996ApJ...461..534L Schade D. et al., Paper IX. =1995ApJ...451L...1S Schade D. et al., Paper X. =1996MNRAS.278...95S Schade D. et al., Paper XI. =1996ApJ...464...79S, Cat. <J/ApJ/464/79> Tresse L. et al., Paper XII. =1996MNRAS.281..847T Galaxies, photometry Galaxies, spectra Redshifts galaxies: distances and redshifts techniques: spectroscopic This paper describes the methods used to obtain the spectroscopic data and construct redshift catalogs for the Canada-France Deep Redshift Survey (CFRS). The full data set consists of more than 1000 spectra, of objects with 17.5=<I_AB_=<22.5, obtained from deep multislit data with the MARLIN and MOS-SIS spectrographs at the Canada-France-Hawaii Telescope (CFHT). The final spectroscopic catalog contains 200 stars, 591 galaxies with secure redshifts in the range 0=<z=<1.3, six QSOs, and 146 objects with very uncertain or unknown redshifts, leading to an overall success rate of identification of 85%. In addition, 67 objects affected by observational problems have been placed in a supplemental list. We describe here the instrumental setup and the observing procedures used to gather this large data set efficiently. New optimal ways of packing spectra on the detector to increase significantly the multiplexing gain offered by multislit spectroscopy are described. Dedicated data reduction procedures have been developed under the IRAF environment to allow for fast and accurate processing. Very strict procedures have been followed to establish a reliable list of final spectroscopic measurements. Fully independent processing of the data has been carried out by three members of the team for each data set associated with a multislit mask, and final redshifts were assigned only after the careful comparison of the three independent measurements. A confidence class scheme was established. We strongly emphasize the benefits of such procedures. Finally, we present the spectroscopic data obtained for 303 objects in the 0000-00 and 1000+25 fields. The success rate in spectroscopic identification is 83% for the 0000-00 field and 84% for the 1000+25 field.
Spectroscopic catalog in the 0000-00 field Spectroscopic catalog in the 1000+25 field CFRS Canada-France Redshift Survey designation --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Imag I_AB_ magnitude number=1 Measured in isophotal aperture; see CFRS I. (1995ApJ...455...50L) mag V-I (V-I)_AB_ colour index number=2 Measured in a 3" aperture; see CFRS I. (1995ApJ...455...50L) mag Q Compactness parameter; see CFRS I. (1995ApJ...455...50L) --- z Redshift --- C Confidence class of spectroscopic identification number=3 See this paper and CRFS III. (1995ApJ...455...75L) In any use of these data, attention should be paid to the confident class that has been assigned to each spectroscopic identification. Identifications with C=<1 are not used in the CFRS scientific analyses described elsewhere. See the text for more information. --- Note *: did correl z=0.3 --- Lam1 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum 0.1nm Cont1 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum --- Lam2 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum 0.1nm Cont2 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum --- Lam3 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum 0.1nm Cont3 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum --- Lam4 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum 0.1nm Cont4 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum --- Lam5 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum 0.1nm Cont5 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum --- Lam6 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum 0.1nm Lam7 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum 0.1nm Lam8 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. C indicates continuum 0.1nm James Marcout, Patricia Bauer CDS 1997 Mar 27 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_455_60.xml The Canada-France redshift survey. III. "Single emission-line" objects, analysis of repeat observations, and spectroscopic identifications in the 1415+52 and 2215+00 fields J/ApJ/455/75 J/ApJ/455/75 CFRS III: 1415+52 and 2215+00 fields The Canada-France redshift survey. III. "Single emission-line" objects, analysis of repeat observations, and spectroscopic identifications in the 1415+52 and 2215+00 fields S J Lilly F Hammer O Le Fevre D Crampton Astrophys. J. 455 75 1995 1995ApJ...455...75L J/ApJ/455/60 : CFRS II: 0000-00 and 1000+25 fields (Le Fevre+ 1995) J/ApJ/455/88 : CFRS IV: 0300+00 field (Hammer+ 1995) J/ApJ/464/79 : CFRS XI: High-redshift field galaxies morphology (Schade+ 1996) Lilly S.J. et al., Paper I. =1995ApJ...455...50L Le Fevre O. et al.. Paper II. =1995ApJ...455...60L, Cat. <J/ApJ/455/60> Hammer F. et al., Paper IV. =1995ApJ...455...88H, Cat. <J/ApJ/455/88> Crampton D. et al., Paper V. =1995ApJ...455...96C Lilly S. J. et al., Paper VI. =1995ApJ...455..108L Hammer F. et al., Paper VII. =1995MNRAS.276.1085H Le Fevre O. et al., Paper VIII. =1996ApJ...461..534L Schade D. et al., Paper IX. =1995ApJ...451L...1S Schade D. et al., Paper X. =1996MNRAS.278...95S Schade D. et al., Paper XI. =1996ApJ...464...79S, Cat. <J/ApJ/464/79> Tresse L. et al., Paper XII. =1996MNRAS.281..847T Galaxies, photometry Galaxies, spectra Redshifts catalogs galaxies: distances and redshifts line: identification This paper is one of a series describing the Canada-France Redshift Survey (CFRS). It is shown how the shape of the continuum around the emission line can be used to distinguish between [O II]{lambda}3727 at z>0.76 and H{alpha} at low redshift in spectra for which only a single isolated emission line is visible. Based on this, [O II]{lambda}3727 is most likely to be the emission line in most of the single emission-line galaxies in the CFRS. The statistics of the repeated observations are analyzed to derive an empirical calibration of the reliability of the spectroscopic identifications in the CFRS in order to determine how often additional observations could lead to the identification of an initially unidentified object and to provide an estimate of the internal velocity accuracy. Finally, the results of spectroscopic observations of 413 objects in the 1415+52 and 2215+00 CFRS survey fields are presented.
Spectroscopic catalog in the 1415+52 field Spectroscopic catalog in the 2215+00 field CFRS Canada-France Redshift Survey designation --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Imag I_AB_ magnitude number=1 Measured in isophotal aperture; see CFRS I. (1995ApJ...455...50L) mag V-I (V-I)_AB_ colour index number=2 Measured in a 3" aperture; see CFRS I. (1995ApJ...455...50L) mag Q Compactness parameter; see CFRS I. (1995ApJ...455...50L) --- z Redshift --- C Confidence class of spectroscopic identification number=3 See this paper and CRFS II. (1995ApJ...455...60L) In any use of these data, attention should be paid to the confident class that has been assigned to each spectroscopic identification. Identifications with C<=1 are not used in the CFRS scientific analyses described elsewhere. See the text for more information. --- Lam1 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line 0.1nm Cont1 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line --- Lam2 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line 0.1nm Cont2 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line --- Lam3 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line 0.1nm Cont3 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line --- Lam4 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line 0.1nm Cont4 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line --- Lam5 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line 0.1nm Cont5 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line --- Lam6 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line 0.1nm Lam7 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line 0.1nm Lam8 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small and a 2 indicates the multiple features of an M star. b indicates break, a for 4863a line 0.1nm James Marcout, Patricia Bauer CDS 1997 Mar 27 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_455_75.xml The Canada-France Redshift Survey. IV. Spectroscopic selection effects and 0300+00 field spectroscopic data. J/ApJ/455/88 J/ApJ/455/88 CFRS IV: 0300+00 field The Canada-France Redshift Survey. IV. Spectroscopic selection effects and 0300+00 field spectroscopic data. F Hammer D Crampton O Le Fevre S J Lilly Astrophys. J. 455 88 1995 1995ApJ...455...88H J/ApJ/455/60 : CFRS II: 0000-00 and 1000+25 fields (Le Fevre+ 1995) J/ApJ/455/75 : CFRS III: 1415+52 and 2215+00 fields (Lilly+ 1995) J/ApJ/464/79 : CFRS XI: High-redshift field galaxies morphology (Schade+ 1996) Lilly S.J. et al., Paper I. =1995ApJ...455...50L Le Fevre O. et al.. Paper II. =1995ApJ...455...60L, Cat. <J/ApJ/455/60> Lilly S.J. et al., Paper III. =1995ApJ...455...75L, Cat. <J/ApJ/455/75> Crampton D. et al., Paper V. =1995ApJ...455...96C Lilly S. J. et al., Paper VI. =1995ApJ...455..108L Hammer F. et al., Paper VII. =1995MNRAS.276.1085H Le Fevre O. et al., Paper VIII. =1996ApJ...461..534L Schade D. et al., Paper IX. =1995ApJ...451L...1S Schade D. et al., Paper X. =1996MNRAS.278...95S Schade D. et al., Paper XI. =1996ApJ...464...79S, Cat. <J/ApJ/464/79> Tresse L. et al., Paper XII. =1996MNRAS.281..847T Galaxies, photometry Galaxies, spectra Redshifts catalogs galaxies: distances and redshifts methods: observational Possible surface brightness selection effects in the redshift catalogs of the Canada-France Redshift Survey are investigated through comparisons of subsamples of the data. Our analyses demonstrate that the securing of redshifts is independent of possible biases arising from surface brightness effects and/or differing galaxy morphologies and orientations. The unusual geometry of the mask designs for our spectroscopic observations also do not produce any significant bias. There is, however, a bias at the highest and lowest redshifts, especially for absorption-line galaxies at z>1 and z<0.2, due to the adopted spectral range (4250-8500A). Apart from the latter, we conclude that our sample of identified galaxies is an unbiased subsample of the original photometric catalog and is essentially limited by I-band flux density (17.5<I_AB_<22.5). Finally, spectroscopic data for the remaining CFRS field is presented. Data for 272 objects in the 0300+0000 field are given.
Spectroscopic catalog in the 0300+00 field CFRS Canada-France Redshift Survey designation --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Imag I_AB_ magnitude number=1 Measured in isophotal aperture; see CFRS I. (1995ApJ...455...50L) mag V-I (V-I)_AB_ colour index number=2 Measured in a 3" aperture; see CFRS I. (1995ApJ...455...50L) mag Q Compactness parameter; see CFRS I. (1995ApJ...455...50L) --- z Redshift --- C Confidence class of spectroscopic identification number=3 See this paper and CRFS II. (1995ApJ...455...60L) In any use of these data, attention should be paid to the confident class that has been assigned to each spectroscopic identification. Identifications with C<=1 are not used in the CFRS scientific analyses described elsewhere. See CFRS II (1995ApJ...455...60L) and CFRS III (1995ApJ...455...75L) for more information. --- Lam1 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small 0.1nm Cont1 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small --- Lam2 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small 0.1nm Cont2 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small --- Lam3 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small 0.1nm Cont3 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small --- Lam4 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small 0.1nm Cont4 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small --- Lam5 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small 0.1nm Cont5 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small --- Lam6 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small 0.1nm Cont6 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small --- Lam7 Spectroscopic feature number=4 Features noted in the spectra. These are largely self-explanatory, except that a 1 indicates that the continuum shape supported the identification in cases in which the number of distinct features was small 0.1nm James Marcout, Patricia Bauer CDS 1997 Mar 27 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_455_88.xml The intermediate stellar mass population in NGC 604 determined from Hubble Space Telescope Images J/ApJ/456/174 J/ApJ/456/174 Intermediate-Mass Population in NGC 604 The intermediate stellar mass population in NGC 604 determined from Hubble Space Telescope Images D A Hunter W A Baum E J O'Neil Jr. R Lynds Astrophys. J. 456 174 1996 1996ApJ...456..174H H II regions Photometry Stars, giant galaxies: individual (M 33) galaxies: photometry galaxies: star clusters galaxies: stellar content HII regions ISM: individual (NGC 604) stars: luminosity function, mass function We present photometry of stars in the giant H II region NGC 604 in M33. The photometry is measured from Hubble Space Telescope images through the F336W, F555W, and F814W broadband filters. Color- magnitude diagrams of the stars in NGC 604 show a main sequence detected down to an M_F555W,0 of -1 (nearly 6M_{sun}_). In addition, there are luminous stars that are probably blue and red supergiants. Based on the previously known presence of Wolf-Rayet stars, we take the age of the cluster to be 3-5Myr. We measure an initial mass function for intermediate-mass stars (6.5-18M_{sun}_) that has a slope of -1.6+/-0.7. This slope is, within the uncertainties, similar to those found for OB associations in the Milky Way and Magellanic Clouds. The density of the luminous stars in NGC 604 is also comparable to that of OB associations in those galaxies even though the total number of stars is greater in NGC 604. A few subclamps have densities that are higher by as much as a factor of 10. A comparison with R136 in the LMC emphasizes that the formation of a large number of massive stars does not necessarily entail a high concentration of those stars.
NGC 604 01 34 32.8 +30 47 04
Photometry Star Star identification number Star identification number. The first significant digit is the chip number; the second is the stellar group number (cluster or background); and the rest is the individual star number. --- X X pixel coord relative to Fig. 1 in paper pix Y Y pixel coord relative to Fig. 1 in paper pix F336W F336W magnitude mag e_F336W F336W magnitude uncertainty mag F555W F555W magnitude mag e_F555W F555W magnitude uncertainty mag F814W F814W magnitude mag e_F814W F814W magnitude uncertainty mag F336W-F555W F336W-F555W color mag e_F336W-F555W F336W-F555W color uncertainty mag F555W-F814W F555W-F814W color mag e_F555W-F814W F555W-F814W color uncertainty mag CDS 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 22-Apr-96 J_ApJ_456_174.xml Sites of relativistic particle acceleration in supernova remnant Cassiopeia A J/ApJ/456/234 J/ApJ/456/234 Cas A radio knots spectral indices Sites of relativistic particle acceleration in supernova remnant Cassiopeia A M C Anderson L Rudnick Astrophys. J. 456 234 1996 1996ApJ...456..234A J/ApJ/441/307 : Proper motions and brightness of Cas A (Anderson+ 1995) Supernova remnants acceleration of particles cosmic rays ISM: individual (Cas A) radiation mechanisms: non-thermal radio continuum: ISM supernova remnants We have determined the synchrotron spectral indices of 304 compact radio knots in the supernova remnant Cassiopeia A. A comparison of these data with the dynamical and brightness properties of these knots tabulated by Anderson & Rudnick (Cat. <J/ApJ/441/307>) indicates that spectral index shows a significant correlation with projected radius from the center of the remnant. Spectrally flat knots reside in a shell coincident with the bright radio ring, while steeper knots occupy a shell coincident with the diffuse radio plateau surrounding the ring. To a lesser extent, we find spectral index to be correlated also with the radio brightness of the knot, in the sense that brighter knots tend to have steeper spectra. No significant correlation is found between spectral index and knot deceleration or rate of brightness change. As the synchrotron spectral index traces the distribution of energy among relativistic particle populations, we use these results to study the nature of particle acceleration mechanisms active in Cas A. Given the dual shell nature of the spectral index distribution in Cas A and the lack of strong correlation between spectral index and dynamical properties of the knots, we conclude that radio-bright compact features are not sites of currently active particle acceleration in Cas A. This conclusion is in agreement with models of supersonic gaseous bullets constructed by Jones, Kang, & Tregillis (1994ApJ...432..194J). In these models, the marked synchrotron brightening which accompanies bullet deceleration is due primarily to preexisting relativistic particles radiating in rapidly amplifying shear-layer magnetic fields, rather than a large infusion of new relativistic particles accelerated in situ. Spectral variations between compact features in Cas A are more likely to reflect modulations in the background particle energy spectra within the remnant, perhaps instilled by temperature variations in the underlying thermal material. This interpretation requires that the diffuse synchrotron emission show the same spectral variations as seen in compact features; preliminary indications suggest that this is the case.
Cas A SN 1680 23 23 12.6 +58 48 48
Radio knot spectral indices (epoch 1987) Knot Knot number --- KnotT Designation number of Tuffs (1986MNRAS.219...13T) --- Xpos Epoch 1987 knot position number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) pix Ypos Epoch 1987 knot position number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) pix BoxX1 Box defining the regression region used for each knot number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) pix BoxY1 Box defining the regression region used for each knot number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) pix BoxX2 Box defining the regression region used for each knot number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) pix BoxY2 Box defining the regression region used for each knot number=1 Positions measured with respect to the optical expansion center at alpha(1950)= 23h21m11s90, delta(1950) = +58deg32'17.6" (Van den Bergh & Kamper 1983ApJ...268..129V) pix alpha Spectral index --- e_alpha rms uncertainty on alpha --- James Marcout, Patricia Bauer CDS 1996 Oct 25 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_456_234.xml Simulation analysis of Ly-Alpha forest spectra. I. Empirical description at z~3 J/ApJ/457/102 J/ApJ/457/102 Ly-Alpha Forest spectra simulation analysis. I. Simulation analysis of Ly-Alpha forest spectra. I. Empirical description at z~3 A Dobrzycki J Bechtold Astrophys. J. 457 102 1996 1996ApJ...457..102D QSOs Spectroscopy cosmology: observations intergalactic medium quasars: absorption lines We present moderate-resolution (~50km/s FWHM) spectra of the Ly-alpha forest for seven quasars with redshifts ranging from 2.53 to 3.13, obtained with the Blue Spectrograph and photon-counting Reticon at the Multiple Mirror Telescope. Combined with spectra of 10 other quasars presented elsewhere, we have characterized the distribution of cloud properties in a way which was designed to minimize any subjective part of the analysis. We used artificial absorption spectra, with the same resolution, sampling and signal-to-noise ratio as a function of wavelength as the actual data. Distributions of the physical parameters of the Ly-alpha clouds, namely, the neutral hydrogen column density (N) and Doppler parameter (b), were approximated with d"N"/dN proportional to N^(-beta) and d"N"/db proportional to exp[-(b-<b>)^2/(2 sigma_b^2)], respectively. We constructed a grid of simulated spectra with different input parameters. Comparison of properties of the simulated spectra with the observed spectra yielded acceptable ranges of parameters. Our technique differs from previous similar work in that we use the information contained in the distribution of the strength of the absorption in each resolution element and the distribution of separations between absorption complexes. We derive beta =1.4+/-0.1 for N ranging from 10^13 to 10^16cm^-2 and <b>=30+/-15km/s. Most previous studies based on line lists indicated beta=1.7-1.9. We attribute this difference to flattening of the column density distribution for low N, recently confirmed by higher resolution observations. Our result for <b>, though consistent with values quoted in the literature, is of lower significance, since it is less than the resolution of our spectra. We conclude by commenting on the importance of line blending in data sets of this kind.
QSO 1206+119 12 09 18 +11 38 31 QSO 1225-017 12 27 59 -02 03 03 QSO 1315+472 QSO 1315+4722 PC 1315+4722 13 18 02 +47 06 30 QSO 1607+183 QSO 1607+1819 16 10 05 +18 11 45 QSO 1623+268 16 25 +26 42 QSO 1700+643 QSO 1700+6414 QSO 1700+642 17 01 00 +64 12 09 QSO 1946+770 QSO 1946+7658 QSO 1946+769 19 44 55 +77 05 52
Line list for Q1206+119 Line list for Q1225-017 Line list for Q1315+472 Line list for Q1607+183 Line list for Q1623+268 Line list for Q1700+643 Line list for Q1946+770 Num Line number --- Lambda Wavelength 0.1nm EW Equivalent width 0.1nm e_EW Equivalent width error 0.1nm Ident Line identification --- Poss Possible line identification --- table2.tex AASTeX version of line lists for all quasars UNKNOWN 1996 Sep 05 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 22-Apr-96 J_ApJ_457_102.xml The stellar halo of M104. I. A survey for planetary nebulae and the planetary nebula luminosity function distance J/ApJ/458/455 J/ApJ/458/455 M 104 planetary nebulae The stellar halo of M104. I. A survey for planetary nebulae and the planetary nebula luminosity function distance H C Ford X Hui R Ciardullo G H Jacoby K C Freeman Astrophys. J. 458 455 1996 1996ApJ...458..455F Planetary nebulae distance scale galaxies: clusters: individual (Virgo) galaxies: distances and redshifts galaxies: individual (M 104) galaxies: stellar content planetary nebulae: general We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.
M 104 NGC 4594 Sombrero Galaxy 12 39 59.3 -11 37 23
M 104 planetary nebulae PNID Identification number of planetary nebula --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec mag m_5007_ magnitude number=1 m_5007_=-2.5log(flux) - 13.74, where "flux" is in erg/cm^2^/s (Ciardullo et al., 1989ApJ...344..715C) mag GSC stars in the M 104 field GSC Identification number from GSC --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Vmag V magnitude mag Secondary reference stars ID Identification number --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec James Marcout, Patricia Bauer CDS 1997 Feb 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_458_455.xml Line strengths and line strength gradients in S0 galaxies J/ApJ/459/110 J/ApJ/459/110 Line strengths and gradients in S0 galaxies Line strengths and line strength gradients in S0 galaxies D Fisher M Franx G Illingworth Astrophys. J. 459 110 1996 1996ApJ...459..110F Galaxies, spectra galaxies: abundances galaxies: elliptical and lenticular, cD galaxies: stellar content Line strengths and their gradients in Mg, Fe, and HBeta have been determined for a sample of 20 S0 galaxies in order to study the stellar populations of their bulges and disks and to investigate their relationship to elliptical galaxies. Data are also presented for the elliptical galaxy NGC 1700 and the E/S0 NGC 3585. We find that S0 galaxies generally follow a similar, though possibly steeper, relationship between central Mg_2 line strength and central velocity dispersion as found for elliptical galaxies. The S0 galaxies show no dependence between Fe line strengths and central velocity dispersion -- similar to the behavior observed in elliptical galaxies. The central Mg/Fe ratios in the luminous S0 galaxies show an overabundance of Mg to Fe with respect to solar element ratios. The magnitudes of the Mg and Fe line-strength gradients within the galaxies are found to be correlated, i.e., objects with steep Mg gradients have correspondingly large Fe gradients. We infer bulge and disk gradients for the nine most edge-on galaxies for which we have both major- and minor-axis profiles. The metal line strengths decrease with radius along the major and minor axes in the bulge-dominated central regions. At larger radii, however, the major-axis metal line strength profiles flatten while the minor-axis bulge profiles fall to lower values. Representative color maps in B-R are presented that display a separation between bulge and disk colors corresponding to the metal line strength profiles. Based on our Mg_2 profiles, the average metal gradient found in the disks of our sub-sample is Delta[Fe/H]/Delta(r/h)=-0.08+/-0.06, which corresponds to a reduction in the mean metallicity of the disk stellar population by <~15% per disk scale length (h). These shallow metallicity gradients are approximately a factor of 2-3 smaller than those derived for the disks of late-type spiral galaxies from H II regions and are consistent with previous investigations that showed a trend for disk metallicity gradients to decrease toward earlier Hubble types. As inferred from our Mg and Fe line strengths, the mean size of the bulge metallicity gradients is Delta[Fe/H]/Delta(log r)=-0.7+/-0.4, which is steeper than typical elliptical galaxy gradients. Our findings do not support formation scenarios in which bulges formed either from heated disk material at late times after disk formation or through dissipationless stellar merging, as neither process includes mechanisms for producing the observed metallicity gradients. Our observations are better explained in terms of formation via dissipative collapse (or merging) at early times.
NGC 1461 03 48.5 -16 23 NGC 1700 04 57.0 -04 52 NGC 2560 08 19.9 +20 59 NGC 3115 10 05.3 -07 44 NGC 3384 10 48.3 +12 38 NGC 3412 10 50.9 +13 25 NGC 3585 11 13.3 -26 45 NGC 3607 11 16.9 +18 03 NGC 3941 11 52.9 +36 59 NGC 3998 11 57.9 +55 27 NGC 4026 11 59.4 +50 58 NGC 4036 12 01.4 +61 54 NGC 4111 12 07.0 +43 03 NGC 4251 12 18.1 +28 11 NGC 4350 12 23.9 +16 42 NGC 4382 12 25.4 +18 11 NGC 4550 12 35.5 +12 13 NGC 4754 12 52.3 +11 19 NGC 4762 12 52.9 +11 14 NGC 5866 15 06.5 +55 45 NGC 6703 18 47.4 +45 33 NGC 936 02 27.6 -01 10
Line strength data Name Object name --- --- Always 'PA=' --- PA Position angle deg n_PA Additional information on PA number=1 For NGC 5866, this column contains 6" N when PA=126deg 6" N and 4.5"NW when PA= 38deg 4.5"NW --- Axis Position angle axis (Minor or Major) --- Rad Radius arcsec Fe4668 =-9.99 Fe4668 line strength estimate --- e_Fe4668 =-9.99 Fe4668 error --- Hbeta =-9.99 Hbeta line strength estimate --- e_Hbeta =-9.99 Hbeta error --- Mgb =-9.99 Mg b line strength estimate --- e_Mgb =-9.99 Mgb error --- Fe5270 =-9.99 Fe5270 line strength estimate --- e_Fe5270 =-9.99 Fe5270 error --- Fe5335 =-9.99 Fe5335 line strength estimate --- e_Fe5335 =-9.99 Fe5335 error --- OIII =-9.99 [O III] line strength estimate --- e_OIII =-9.99 OIII error --- Mg2 data Name Object name --- --- Always ' PA=' --- PA Position angle deg n_PA Additional information on PA number=1 For NGC 5866, this column contains 6" N when PA=126deg 6" N and 4.5"NW when PA= 38deg 4.5"NW --- Axis Position angle axis (Minor or Major) --- Rad Radius arcsec Mg2 Mg_2 line strength estimate --- e_Mg2 Mg2 error --- Patricia Bauer CDS 1996 Sep 06 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 22-Apr-96 J_ApJ_459_110.xml Opening a new window on Ap star atmospheres: a T-Tauri relation for HR 3831 from its limb-darkened pulsation amplitudes J/ApJ/459/278 J/ApJ/459/278 Photometry of HD 3831 Opening a new window on Ap star atmospheres: a T-Tauri relation for HR 3831 from its limb-darkened pulsation amplitudes J M Matthews W H Wehlau J Rice G A H Walker Astrophys. J. 459 278 1996 1996ApJ...459..278M Photometry Photometry, infrared Stars, Ap stars: atmospheres stars: individual (HR 3831) stars: oscillations stars: peculiar We demonstrate a new approach for probing the atmospheres of selected chemically peculiar magnetic stars. Using the Cerro Tololo Inter-American Observatory (CTIO) 1.0 and 1.5m telescopes simultaneously on two nights in 1991, we obtained optical and infrared high-speed photometry of the rapidly oscillating Ap (roAp) star HR 3831 (=HD 83368), which pulsates with a period of ~11.8 minutes. Oscillation amplitudes (or upper limits) in each of eight bandpasses were measured by Fourier analysis, revealing the very steep decline in amplitude with increasing wavelength characteristic of roAp stars. Matthews and coworkers have shown that this can be explained by the wavelength dependence of limb darkening and its filtering effect on the integrated amplitude of an (l,m)=(1,0) nonradial pulsation mode. Since the eigenfrequency spectrum of HR 3831 is dominated by just such a dipole mode, it is possible to infer limb-darkening coefficients beta(lambda) for its atmosphere from our amplitude measurements. These coefficients are used to derive a source function through the Eddington-Barber relation, which leads to a relation for temperature versus optical depth in the stellar photosphere. Our results show that the T-Tau(5000) curve is much steeper for HR 3831 than for the Sun (at least at the rotational phase when the star's magnetic pole dominates the visible hemisphere). We also calculate the gradient dT/dtau as a function of wavelength to compare with the curve expected for H- continuous opacity. This type of diagnostic may become a useful tool for checking the predictions of diffusion theory.
HR 3831 HD 83368 09 36 25.3 -48 45 04
Differential photometry, b bandpass Differential photometry, v bandpass Differential photometry, y bandpass Differential photometry, R bandpass Differential photometry, I bandpass Differential photometry, J bandpass Differential photometry, H bandpass Differential photometry, K bandpass HJD-2448000 Heliocentric Julian Date - 2448000 d dMag Differential magnitude normalized to the mean mag CDS 1996 Sep 06 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 22-Apr-96 J_ApJ_459_278.xml The distances of planetary nebulae and the galactic bulge J/ApJ/459/606 J/ApJ/459/606 Distances of planetary nebulae The distances of planetary nebulae and the galactic bulge S E Schneider D Buckley Astrophys. J. 459 606 1996 1996ApJ...459..606S V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) Morphology Planetary nebulae Radio lines circumstellar matter Galaxy: center planetary nebulae: general radio continuum: ISM We describe an improved method for determining the distances of planetary nebulae (PNe) based on a theoretical/empirical relationship between their radii and radio surface brightness. Like the Shklovsky (constant mass) distance method, our relationship requires only radio flux density and angular size measurements, which are widely available in the literature. Based on models matching the overall Galactic distribution of PNe, we determine how PNe observed in the direction of the Galactic center are actually distributed relative to the bulge in order to establish the usefulness of these PNe for distance studies. We then use the bulge PNe along with PNe with independent distances to establish, calibrate, and test the accuracy of the method. When compared to the best available data our distance method appears to yield distance errors consistent with a scatter of <25% (1{sigma}). And, based on our models scaled to local PNe, we find a mean Galactic center distance of 8.3+/-2.6kpc for the bulge PNe. The relationship that PNe exhibit between radius and surface brightness is in excellent agreement with our simulated nebulae from Paper I (Buckley & Schneider, 1995ApJ...446..279B). We find that no simple power law can describe the changing mass and radius of a PN as it ages; however, our empirical relationship has a limiting behavior that is almost indistinguishable from the assumption made in Shklovsky's distance method that PNe have a constant ionized mass. We reexamine the dispute about the validity of the Shklovsky's distance method as applied to Galactic center PNe in light of these results, and we argue that the Shklovsky method does predict the distances of large, low surface brightness PNe well, but it increasingly overestimates the distance of smaller PNe.
Radio flux densities and sizes of Galactic Center PNe PN PN designation --- S6cm Flux density at 6cm (5GHz) mJy l_Diamph Limit flag on Diamph --- Diamph Photographic diameter from the Strasbourg-ESO catalogue (Cat. <V/84>) arcsec u_Diamph Uncertainty flag on Diamph --- n_Diamph Note on Diamph number=1 s: stellar ): indicates that the source shows significant discrepancies between radio and photographic measurements --- l_Diam Limit flag on Diam --- Diam Adopted metric diameter arcsec n_Diam Note on Diam number=1 s: stellar ): indicates that the source shows significant discrepancies between radio and photographic measurements --- James Marcout, Patricia Bauer CDS 1997 Apr 10 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_459_606.xml Energy Deposition and Photoelectric Emission from the Interaction of 10 eV to 1 MeV Photons with Interstellar Dust Particles J/ApJ/459/686 J/ApJ/459/686 Energy Deposition in Interstellar Dust Grains Energy Deposition and Photoelectric Emission from the Interaction of 10 eV to 1 MeV Photons with Interstellar Dust Particles E Dwek R K Smith Astrophys. J. 459 686 1996 1996ApJ...459..686D http://adsabs.harvard.edu/article_service.html for source reference.Laor, A., Draine, B.T. 1993, ApJ 402, 441 =1993ApJ...402..441L Extinction Interstellar medium Opacities This catalog contains calculated tables of the energy deposition into dust grains by photons with energies between 10 eV and 1 MeV. The tables give the deposition for 60 different energies and 15 dust grain sizes. Tables for both silicate and graphite grains are presented. Photoelectric absorption, auger electrons, and Compton scattering are used in the calculations, which were done with a Mie code when necessary and a particle approach when appropriate. The file graphite.dat corresponds to Table 5.1 in the source reference. Silicate.dat corresponds to Table 5.2.
</tableLink> <tableLink xlink:href="silicate.dat"> <title>Deposition in silicate Ephot Energy of incoming photon eV E5nm Energy deposition*Q_abs for grain size=5nm These fields contain the energy deposition multiplied by Q_abs. Where Q_abs is the dust absorption efficiency calculated from Mie theory. The grain size indicated is the dust particle radius. The total energy deposited in a dust particle of radius a is therefore flux * pi a^2 * dt * table_value; the flux has units of photons per cm^2 per second, pi a^2 is the geometric area of the dust, dt is the length of time considered, and the table value contains both Q_abs (which when multiplied by the geometric cross section gives the cross section for absorption) and the energy deposited when that photon is absorbed, which may be the entire photon's energy or some lesser value. -------------------------------------------------------------------------------- Acknowledgements: The authors thank James Rathkopf and Rick Cullen from LLNL for the Auger data, Peter Martin for the UV optical constants, and Alice Trenholm, David Stoutamire, and Ari Laor for useful conversations. The ADC thanks author R. Smith for providing the data and the original ReadMe document. eV E7nm Energy deposition*Q_abs for grain size=7nm eV E10nm Energy deposition*Q_abs for grain size=10nm eV E15nm Energy deposition*Q_abs for grain size=15nm eV E20nm Energy deposition*Q_abs for grain size=20nm eV E30nm Energy deposition*Q_abs for grain size=30nm eV E50nm Energy deposition*Q_abs for grain size=50nm eV E70nm Energy deposition*Q_abs for grain size=70nm eV E100nm Energy deposition*Q_abs for grain size=100nm eV E150nm Energy deposition*Q_abs for grain size=150nm eV E200nm Energy deposition*Q_abs for grain size eV E300nm Energy deposition*Q_abs for grain size=300nm eV E500nm Energy deposition*Q_abs for grain size=500nm eV E700nm Energy deposition*Q_abs for grain size=700nm eV E1um Energy deposition*Q_abs for grain size=1micron eV Randall Smith NASA/GSFC & James Gass SSDOO/ADC 1997 Jul 10 UNKNOWN UNKNOWN 9-July-1997 As submitted, the first record of each data file contained a header record. These were removed to conform with CDS/ADC standards. R. Smith's ReadMe was modified by J. Gass [SSDOO/ADC] to include a byte-by-byte table and additional features of a standard document. J_ApJ_459_686.xml The Einstein Two-Sigma Catalog J/ApJ/461/127 J/ApJ/461/127 The Einstein Two-Sigma Catalog The Einstein Two-Sigma Catalog E C Moran D J Helfand R H Becker R L White Astrophys. J. 461 127 1996 1996ApJ...461..127M VII/152 : Einstein Medium Sensitivity Survey Catalog Moran, E.C., Helfand, D.J., Becker, R.H., White, R.L. 1996: ApJ. 461, 127. X-ray sources The X-ray sources from the observations with the Einstein Observatory (HEAO-2) with intensities of 2-sigma above the background are compiled in this catalog. This catalog covers more sky at fainter flux levels than the Einstein Medium Sensitivity Survey. Fields with diffuse emission sources were excluded. Thus data within 10 degrees of the galactic plane as well as fields within the boundaries of the Magellanic Clouds were excluded. The catalog covers 1850 sq. degrees of the sky. The generation of the Einstein Two-Sigma Catalog was described in detail by Moran et al. (1996). Read this article carefully to ensure responsible use of the Catalog. Address any questions to Ed Moran (edhed@igpp.llnl.gov). In particular it should be noted that only 28%, or about 13,000 sources in the 2-sigma catalog are real sources. The authors show that cross-correlations with other catalogs is an effective way to select sources in this catalog that are probably real.
HEAO-2
The 2-sigma catalog RAh RA (1950) of the source h RAm RA (1950) of the source min RAs RA (1950) of the source s DE- Sign Declination (1950) --- DEd Dec (1950) of the source deg DEm Dec (1950) of the source arcmin DEs Dec (1950) of the source arcsec S/N Signal-to-noise ratio of the source Signal-to-noise ratio of the source, based on the counts collected within a 1.25 arcmin radius circular aperture. --- IPCSEQ IPC Sequence number containing the source --- cnts125 Number of background-subtracted counts collected within a 1.25 arcmin radius circular aperture The number of background-subtracted counts contained in the source, collected within circular apertures of radii 1.25 and 2.0 arcmin. arcmin-2 cnts20 Number of background-subtracted counts collected within a 2.0 arcmin radius circular aperture arcmin-2 exp125 flatfield-weighted exposure time for the source in the 1.25 arcmin radius aperture The flatfield-weighted exposure time (sec) for the source in the 1.25 and 2.0 arcmin radius apertures. s exp20 flatfield-weighted exposure time for the source in the 2.0 arcmin radius aperture s N125 Number of "good" pixels used for count in the 1.25 arcmin radius aperture The number of ``good'' pixels used to accumulate counts for the source in the 1.25 arcmin and 2.0 arcmin radius apertures and for the background in the concentric 3-6 arcmin radius annulus. The edges of the IPC, its window support ribs, or pixel deletions resulting from the detection of brighter nearby sources can cause these numbers to be less than their maximum values of 21, 45, and 304. At least 15 of the 21 pixels in the 1.25 arcmin aperture had to be unshadowed and undeleted for a source to to be included in the Catalog. --- N20 Number of "good" pixels used for count in the 2.0 arcmin radius aperture --- Nbg Number of "good" pixels used for the background count in the concentric 3-6 arcmin radius annulus --- Paul Kuin NASA/ADC 1997 Mar 12 J_ApJ_461_127.xml Planetary nebulae as standard candles. X. Tests in the Coma I region. J/ApJ/462/1 J/ApJ/462/1 PNe in the Coma I region Planetary nebulae as standard candles. X. Tests in the Coma I region. G H Jacoby R Ciardullo W E Harris Astrophys. J. 462 1 1996 1996ApJ...462....1J Nebulae, planetary distance scale galaxies: clusters: individual (Coma I) We present the result of an [OIII]500.7nm survey for planetary nebulae (PNe) in three galaxies of the Coma I group: NGC 4278 (Hubble type E1), NGC 4494 (E1), and NGC 4565 (edge-on Sb). Using the planetary nebula luminosity function (PNLF), we derived distances to NGC 4494 (12.8+/-0.9Mpc), NGC 4564 (10.5^+0.8^_-1.0_Mpc), and NGC 4278 (10.2^+0.7^_-1.0_Mpc). The larger distance for NGC 4494 is significant beyond the 99% confidence level when the common systematic errors in all three distances are removed. This agrees with the results of the globular cluster luminosity function and surface brightness fluctuation methods, both of which place NGC 4565 in front of NGC 4494. The large separation is also consistent with the results of Virgocentric flow models, which predict triple-valued solutions to the Hubble flow in that direction.
NGC 4278 planetary nebulae NGC 4494 planetary nebulae ID ID number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Rad Isophotal radius from galaxy arcmin m5007 Lambda5007 magnitude (m5007=-2.5logF5007 - 13.74) mag Note Note number=1 S when PNe that are part of the statistical samples --- NGC 4565 planetary nebulae ID ID number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec z PN distance from galactic plane arcsec m5007 Lambda5007 magnitude (m5007=-2.5logF5007 - 13.74) mag Note S when PNe that are part of the statistical samples --- Astrometric reference stars Name Galaxy name --- ID Star identification --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Patricia Bauer CDS 1996 Sep 06 Robin Ciardullo <rbc@astro.psu.edu> J_ApJ_462_1.xml A deep multicolor survey. II. Initial spectroscopy and comparison with expected quasar number counts. J/ApJ/462/614 J/ApJ/462/614 A deep multicolor survey. II. A deep multicolor survey. II. Initial spectroscopy and comparison with expected quasar number counts. P B Hall P S Osmer R F Green A C Porter S J Warren Astrophys. J. 462 614 1996 1996ApJ...462..614H J/ApJS/104/185 : A deep multicolor survey. I. (Hall+ 1996) Galaxies, photometry QSOs Surveys catalogs galaxies: photometry quasars: general surveys We have used the Kitt Peak National Observatory 4m Mayall telescope to image 0.83 square degrees of sky in six fields at high galactic latitude in six filters spanning 3000-10000A to magnitude limits ranging from 22.1 to 23.8. As a first use of this database, we have conducted a multicolor survey for quasars. We discuss various methods of selecting outliers in different color-color diagrams and multicolor space that have been used to identify quasars at all redshifts from their colors alone. We discuss the initial results of our program of spectroscopic identification which has so far resulted in the identification of over 40 faint quasars, including one a z>4, a similar number of compact narrow emission-line galaxies, and a number of unusual and potentially interesting stars. We use these spectroscopic results, along with extensive simulations of quasar spectra, to study the efficiency of our candidate selection procedures. Finally, we compare the number counts of our quasars and quasar candidates to the expected numbers based on previous studies of the quasar luminosity function. The agreement of our observations with these expectations is good in most cases. However, we do estimate that our survey contains more quasars with B<21 and z<2.3 than expected from the results published by Koo & Kron in (1988ApJ...325...92K) and more z>3 quasars than expected from the results published by Warren, Hewett & Osmer in (1994ApJ...421..412W), both at the 3 {sigma} level. Additional spectroscopic observations will be required to confirm or refute these excesses.
Quasars: identification Compact narrow emission-line galaxies: identifications No Sequential number --- Name DMS or N designation number=1 DMS followed by the epoch 1950.0 position in table1, N followed by the epoch 1950.0 position in table2. --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Bmag B magnitude mag z Redshift --- u_z Uncertainty flag on z --- Notes Notes --- table1.tex LaTeX version of table1 table2.tex LaTex Version of table2 Patricia Bauer CDS 1996 Oct 03 Pat Hall <pathall@as.arizona.edu> J_ApJ_462_614.xml The Extragalactic Distance Scale Key Project. III. The discovery of Cepheids and a new distance to M101 using the Hubble Space Telescope. J/ApJ/463/26 J/ApJ/463/26 Extragalactic Distance Scale Key Project. III The Extragalactic Distance Scale Key Project. III. The discovery of Cepheids and a new distance to M101 using the Hubble Space Telescope. D D Kelson G D Illingworth W L Freedman J A Graham R Hill B F Madore A Saha P B Stetson R C Kennicutt Jr. J R Mould S M Hughes L Ferrarese R Phelps A Turner K H Cook H Ford J G Hoessel J Huchra Astrophys. J. 463 26 1996 1996ApJ...463...26K Photometry Stars, variable Cepheids distance scale galaxies: distances and redshifts galaxies: individual (M 101) We report on the discovery of 29 Cepheid variables in the galaxy M101 using the original Wide Field Camera (WFC) and the new Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope. We observed a field in M101 at 17 independent epochs in V (F555W), five epochs in I (F785LP/F814W), and one epoch in B (F439W), with a time interval baseline of 381 days. We have found Cepheids with periods ranging from 10 to 60 days. The data have been calibrated using WFPC2 observations with zero points derived from Omega Cen, Pal 4, and NGC 2419 observations. This calibration has been verified by using the Medium Deep Survey (MDS) WFC photometric zero points, and ground-based secondary standards in V and I. The V calibrations agree to +/-0.06mag, and the I calibrations agree to +/-0.4mag. We have constructed V and I period-luminosity (PL) relations and have derived apparent distance moduli based on a distance modulus for the Large Magellanic Cloud (LMC) of 18.50mag and a reddening of E(B-V)=0.10mag to the LMC Cepheids. Period-residual minimization was used to minimize the effects of Malmquist bias on the period-luminosity relation fitting process. Using a Galactic extinction law and the apparent V and I distance moduli, we have found a mean reddening for the M101 sample of E(B-V)=0.03mag and a true distance modulus to M101 of 29.34+/-0.17mag, corresponding to a distance of 7.4+/-0.6Mpc. The sources of error have been rigorously tracked through an error budget; systematic and random errors contribute roughly equally to the quoted error. The mean gas-phase metal abundances in the LMC and in the M101 outer field are similar so we expect metallicity effects to be minimal. These Cepheids will be used in conjunction with results from a Key Project search for Cepheids in an inner field, where the metallicity is larger by a factor of 5, to probe the effects of abundance on the Cepheid period-luminosity relation.
HST
V photometry Cepheid Cepheid number --- Per Period d JD Julian date, midpoint of individual exposure d CCD Which CCD the star can be found in --- Xpos X position on CCD frame pix Ypos Y position on CCD frame pix Vmag Calibrated F555W magnitude mag e_Vmag ALLFRAME uncertainty in F555W magnitude mag I photometry Cepheid Cepheid number --- Per Period d JD Julian date, midpoint of individual exposure d CCD Which CCD the star can be found in --- Xpos X position on CCD frame pix Ypos Y position on CCD frame pix Imag Calibrated F814W magnitude mag e_Imag ALLFRAME uncertainty in F814W magnitude mag Patricia Bauer, CDS 1997 Jan 31 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 10-Oct-96 J_ApJ_463_26.xml Canada-France Redshift Survey. XI. Morphology of high-redshift field galaxies from high-resolution ground-based imaging J/ApJ/464/79 J/ApJ/464/79 CFRS XI: High-redshift field galaxies morphology Canada-France Redshift Survey. XI. Morphology of high-redshift field galaxies from high-resolution ground-based imaging D Schade S J Lilly O Le Fevre F Hammer D Crampton Astrophys. J. 464 79 1996 1996ApJ...464...79S J/ApJ/455/60 : CFRS II: 0000-00 and 1000+25 fields (Le Fevre+ 1995) J/ApJ/455/75 : CFRS III: 1415+52 and 2215+00 fields (Lilly+ 1995) J/ApJ/455/88 : CFRS IV: 0300+00 field (Hammer+ 1995) Lilly S.J. et al., Paper I. =1995ApJ...455...50L Le Fevre O. et al.. Paper II. =1995ApJ...455...60L, Cat. <J/ApJ/455/60> Lilly S.J. et al., Paper III. =1995ApJ...455...75L, Cat. <J/ApJ/455/75> Hammer F. et al., Paper IV. =1995ApJ...455...88H, Cat. <J/ApJ/455/88> Crampton D. et al., Paper V. =1995ApJ...455...96C Lilly S. J. et al., Paper VI. =1995ApJ...455..108L Hammer F. et al., Paper VII. =1995MNRAS.276.1085H Le Fevre O. et al., Paper VIII. =1996ApJ...461..534L Schade D. et al., Paper IX. =1995ApJ...451L...1S Schade D. et al., Paper X. =1996MNRAS.278...95S Tresse L. et al., Paper XII. =1996MNRAS.281..847T Galaxies, photometry Morphology Redshifts galaxies: distances and redshifts galaxies: evolution galaxies: photometry The 143 galaxies with secure redshifts (Z_median_=0.62) from the 1415+52 field of the Canada-France Redshift Survey have been imaged with median seeing of 0.67" (FWHM). Structural parameters have been derived by fitting multicomponent models and the results confirm two phenomena seen in a smaller sample of galaxies imaged with the Hubble Space Telescope. First, 11+/-3% of the galaxies lie off the normal locus of color versus bulge fraction B/T. This class of objects ("blue nucleated galaxies," or BNGs) was identified using HST observations (Schade et al. 1995ApJ...451L...1S, hereafter CFRS IX), and it was shown that they are associated with peculiar/asymmetric structure and merger/interactions. The observed frequency of BNGs in this sample is 14+/-4% 0.5<z<1.2 and 6^+6^_-3_% at 0.2<z<0.5, but the true frequency is likely to be a factor ~2 higher after corrections are made for the effect of asymmetric/peculiar structures. Galaxy disks at 0.5<z<1.1 are found to have a mean rest-frame, inclination-corrected central surface brightness of {mu}_AB_(B)=19.8+/-0.1mag/arcsec^2^, ~1.6mag brighter than the Freeman (1970ApJ...160..811F) value. At low redshift (0.2<z<0.5) the mean surface brightness [{mu}_AB_(B)=21.3+/-0.25] is consistent with the Freeman value. These results are consistent with the HST observations. With larger numbers of galaxies and therefore more statistical weight they demonstrate the capabilities, and limits, of ground-based work in the study of galaxy morphology at high redshift.
Canada-France Redschift Survey Galaxies at z>0.5 CFRS Canada-France Redshift Survey designation --- z Redshift --- Imag I_AB_ magnitude mag V-I (V-I)_AB_ colour index mag MBmag Absolute B_AB_ magnitude number=1 Absolute magnitudes assume H_0_=50km/s/Mpc, q_0_=0.5 mag U-V (U-V)_AB_ colour magnitude mag B/T Colour versus bulge fraction --- h Scale length kpc James Marcout, Patricia Bauer CDS 1997 Mar 27 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_464_79.xml Radio Recombination Lines from Inner Galaxy Diffuse Gas. II. The Extended Low-Density Warm ionized Medium and the "Worm-Ionized Medium" J/ApJ/466/191 J/ApJ/466/191 Low-Density Warm Ionized Medium Radio Recombination Lines from Inner Galaxy Diffuse Gas. II. The Extended Low-Density Warm ionized Medium and the "Worm-Ionized Medium" C Heiles W T Reach B -C Koo Astrophy. Jour. 466 19 1996 1996ApJ...466..191H H II regions Interstellar medium Radio lines These data characterize the extended low-density warm ionized medium (the ELDWIM). The file contains results from a Radio Recombination Line survey of the inner Galaxy at 583; emission was observed at 418 points.
The measurements GLON Galactic longitude deg GLAT Galactic latitude deg Tb Line intensity mK ul_Tb Approximate upper limit of T_b mK FWHM FWHM velocity range km/s vel_lsr Velocity with respect to the lsr km/s n_Tb Comments GB = observation was made at NRAO HC = observation was made at HCRO Sxx = position is close to Sharpless HII region xx ic = spectrum has i Gaussian components W = detection is weak note 1 = Spectra plotted and discussed in HKLR (Heiles et al. 1995) note 2 = This spectrum (l,b) = (31.50, -3.00) has an extraordinarily wide Gaussian. It may be more appropriately fitted by two Gaussian with (Tb, FMHM, Vlsr) = (6.3, 53.5, 44.2) and (6.6, 36.2, 105.0) but the signal/noise does not warrant these extra parameters. --- N. G. Roman SSDOO/ADC 1997 May 27 J_ApJ_466_191.xml Adaptive optics near-infrared imaging of R136 in 30 Doradus: the stellar population of a nearby starburst. J/ApJ/466/254 J/ApJ/466/254 NIR Imaging of R136 in 30 Dor Adaptive optics near-infrared imaging of R136 in 30 Doradus: the stellar population of a nearby starburst. B Brandl B J Sams F Bertoldi A Eckart R Genzel S Drapatz R Hofmann M Loewe A Quirrenbach Astrophys. J. 466 254 1996 1996ApJ...466..254B Photometry, UVBRIJKLMNH Stars, dwarfs HII regions infrared: stars ISM: individual (30 Dor) Magellanic Clouds stars: early-type techniques: image processing We report 0.15" resolution near-infrared (NIR) imaging of R136, the central region of 30 Doradus in the Large Magellanic Cloud. Our 12.8"x12.8" images were recorded with the MPE camera SHARP II at the 3.6m ESO telescope, using the adaptive optics system COME ON+. The high spatial resolution and sensitivity (20th magnitude in K) of our observations allow our H- and K-band images to be compared and combined with recent Hubble Space Telescope (HST) WFPC2 data of R136. We fit theoretical models with variable foreground extinction to the observed magnitudes of ~1000 stars (roughly half of which were detected in HST and NIR bands) and derive the stellar population in this starburst region. We find no red giants or supergiants; however, we detect ~110 extremely red sources which are probably young, pre-main-sequence low- or intermediate-mass stars. We obtained narrow-band images to identify known and new Wolf-Rayet stars by their He II (2.189um) and BrGamma (2.166um) emission lines. The presence of W-R stars and absence of red supergiants narrow the cluster age to 3-5Myr, while the derived ratio of W-R to O stars of 0.05 in the central region favors an age of ~3.5Myr, with a relatively short starburst duration. For the O stars, the core radius is found to be 0.1pc and appears to decrease with increasing stellar mass. The slope of the mass function is Gamma=-1.6 on average, but it steepens with increasing distance from the cluster center from Gamma=-1.3 in the inner 0.4pc to Gamma=-2.2 outside 0.8pc for stars more massive than 12 Msun. The radial variation of the mass function reveals strong mass segregation that is probably due to the cluster's dynamical evolution.
The 971 main sequence stars in our field of view (YSO candidates and WR stars were excluded) Star Star number from Hunter et al. (1995ApJ...488..179H) --- Xpos X position on detector (512x512 grid) pix Ypos Y position on detector (512x512 grid) pix Umag =-99.99 U magnitude The U, V & I band magnitudes were converted from WFPC2 magnitudes according the the relations in Hunter et al. (1995ApJ...488..179H). Extinction was not taken into account. mag Vmag =-99.99 V magnitude mag Imag =-99.99 I magnitude mag Hmag =-99.99 H magnitude The H & K magnitudes were derived from the authors' observations with adaptive optics. Extinction is not taken into account. mag Kmag =-99.99 K magnitude mag CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 22-Oct-96 J_ApJ_466_254.xml Spectroscopic orbits for three binaries with low-mass companions and the distribution of secondary masses near the substellar limit J/ApJ/466/415 J/ApJ/466/415 Spectroscopic orbits for three binaries Spectroscopic orbits for three binaries with low-mass companions and the distribution of secondary masses near the substellar limit T Mazeh D W Latham R P Stefanik Astrophys. J. 466 415 1996 1996ApJ...466..415M Binaries, spectroscopic Radial velocities binaries: spectroscopic stars: individual (HD 29587, HD 114762, HD 140913) stars: low-mass, brown dwarfs We present orbital solutions for three low-amplitude spectroscopic binaries discovered in a sample of 20 solar-type IAU radial velocity standard stars observed with the Digital Speedometers at the Harvard- Smithsonian Center for Astrophysics. We update the orbital solutions for HD 114762 and HD 140913, and present a preliminary new solution for HD 29587. For all three orbits, the minimum mass for the secondary is less than 0.08M_{sun}_, the borderline between stellar and substellar masses. We consider the probability that all three binaries have small enough inclination angles so that their companions are above the substellar limit. To do so, we treat the 20 IAU standards as a sample drawn from a population of binaries with a mass-ratio distribution that does not allow any substellar companions. We calculate the probability that such a sample could still have three binaries, with the low-amplitude orbits actually found within the IAU sample. We show that this probability is small, depending on the specific mass-ratio distribution. For example, a flat mass-ratio distribution that assumes there are no substellar companions can be excluded at a high confidence level, 99.7%. We further show that our three detections may imply that the secondary-mass distribution rises near the substellar limit. However, the observations do not yet allow us to distinguish whether the unseen companions of HD 114762, HD 140913, and HD 29587 have stellar or substellar masses. In particular, recent attempts to estimate the mass of the companion of HD 114762 based on assumptions about the intrinsic rotation of the primary are inconclusive, and the companion could easily have a mass as low as 0.02M_{sun}_. We compare our three detections with the null results of four very precise radial velocity searches for substellar companions. The difference is indeed puzzling but can be accounted for if just a small fraction of the solar-type stars, of the order of a few percent, have companions with masses near the substellar limit.
HD 29587 04 41 33.9 +42 07 28 HD 114762 13 12 21.7 +17 31 01 HD 140913 15 45 07.7 +28 28 10
Individual velocities HD Henry Draper Catalog number (Cat. <III/135>) --- RAh Right ascension, J2000 h RAm Right ascension, J2000 min RAs Right ascension, J2000 s DE- Declination sign --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec HJD Heliocentric Julian Date d RV Barycentric radial velocity km/s e_RV Internal estimate of velocity error km/s TDR Tonry-Davis (1979AJ.....84.1511T) R value --- CC Peak value of the correlation coefficient --- CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 22-Oct-96 J_ApJ_466_415.xml The intermediate stellar mass population in the M31 OB association NGC 206. J/ApJ/468/633 J/ApJ/468/633 Photometry in the M31 OB association NGC 206 The intermediate stellar mass population in the M31 OB association NGC 206. D A Hunter W A Baum E J O'Neil Jr. R Lynds Astrophys. J. 468 633 1996 1996ApJ...468..633H J/ApJS/98/595 : OB associations in M31 (Hill+ 1995) Associations, stellar Photometry galaxies: individual: M 31 galaxies: star clusters galaxies: stellar content Hertzsprung-Russell diagrams open clusters and associations: individual: NGC 206 As part of our effort to determine what affects the star formation process by looking at the products of that process, we have obtained broadband Hubble Space Telescope images of the large OB association NGC 206 in the nearby spiral galaxy M31. Our images cover approximately the southern half of the association. We have detected stars down to an F555W magnitude of 25.5 and measure stars on the main sequence in NGC 206 to an M_F555W,0_ of -1 or a mass of ~6M_{sun}_. From a comparison with isochrones, ages up to about 8Myr are plausible, and we adopt an age of 6Myr. For stellar masses 6-15M_{sun}_, we determine an initial mass function slope of -1.4+/-0.5. This is close to the value for a Salpeter mass function, although the uncertainty is large. The uncertainty in the slope represents disagreement among the individual mass bins. In terms of intermediate-mass stars (6-15M_{sun}_) the NGC 206 star formation event appears to be typical of star formation processes in other nearby galaxies, and it is part of a growing number of studies ,that are finding similarities in the products of the star formation processes in a wide variety of star formation events and galactic environments. Nevertheless, the density of stars formed in NGC 206 is much lower than that in giant H II regions such as NGC 604 in M33 or 30 Doradus in the LMC and in typical OB associations.
HST NGC 206 00 37 50.3 +40 27 54
Cluster photometry Background field photometry ID Star identification number --- xpos x pixel coordinate number=1 1 pix = 0.1". The region is centered near: RA=00h40m28s, DE=+40{deg}44.0' (2000), in table2.dat RA=00h40m51s, DE=+40{deg}41.3' (2000), in table3.dat pix ypos y pixel coordinate number=1 1 pix = 0.1". The region is centered near: RA=00h40m28s, DE=+40{deg}44.0' (2000), in table2.dat RA=00h40m51s, DE=+40{deg}41.3' (2000), in table3.dat pix F336W F336W magnitude number=2 A magnitude of 100.00 indicates that the star was not measured through that filter. mag e_F336W uncertainty in F336W magnitude number=2 A magnitude of 100.00 indicates that the star was not measured through that filter. mag F555W F555W magnitude mag e_F555W uncertainty in F555W magnitude mag F814W F814W magnitude mag e_F814W uncertainty in F814W magnitude mag F336W-F555W F336W-F555W color number=2 A magnitude of 100.00 indicates that the star was not measured through that filter. mag e_F336W-F555W uncertainty in F336W-F555W color number=2 A magnitude of 100.00 indicates that the star was not measured through that filter. mag F555W-F814W F555W-F814W color mag e_F555W-F814W uncertainty in F555W-F814W color mag Patricia Bauer CDS 1998 Sep 11 Brian Skiff <bas@lowell.Lowell.Edu> J_ApJ_468_633.xml The UV-brightest stars of M33 and its nucleus: discovery, photometry, and optical spectroscopy J/ApJ/469/629 J/ApJ/469/629 UV-brightest stars of M33 and its nucleus The UV-brightest stars of M33 and its nucleus: discovery, photometry, and optical spectroscopy P Massey L Bianchi J B Hutchings T P Stecher Astrophys. J. 469 629 1996 1996ApJ...469..629M Photometry, UBV Photometry, ultraviolet galaxies: individual (M 33) galaxies: stellar content stars: early-type stars: Wolf-Rayet ultraviolet: stars We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti & Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.
ASTRO 1/UIT
UIT sources in M33 Star Source name --- RAh Right ascension, J2000 h RAm Right ascension, J2000 min RAs Right ascension, J2000 s DE- Declination sign, always blank --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec N3 Number of stars within 3" of V counterpart Total number of stars found on V image within 3" of the UIT V counterpart position. --- N5 Number of stars within 5" of V counterpart Total number of stars found on V image within 5" of the UIT V counterpart position. --- FUV FUV magnitude mag FUV-NUV FUV-NUV color mag Vmag V magnitude mag U-B U-B color index mag B-V B-V color index mag FUV-V FUV-V color index mag Sp Spectral type --- Comment Comments, cross IDs, indication of crowding Cross-identifications given in the Comments are: Halpha designation is from the unpublished Halpha survey described by Neese et al. (1991, IAU Symp. 143), the full text of which is in preparation B: stars from the list of blue stars in M33 by Humphreys & Sandage, 1980ApJS...44..319H. HSanon: unlisted blue stars on their finding charts, which also form the basis of describing a star as being inside a given OB association. obnn-xxx: stars from Massey et al., 1995AJ....110.2715M (Cat. <J/AJ/110/2715>) MC: refers to Massey & Conti, 1983ApJ...273..576M, W-R stars CM: refers to Conti & Massey, 1981ApJ...249..471C, stars in H II regions W91: refers to stars listed by Wilson, 1991AJ....101.1663W AM: stars are W-R stars found by Armandroff & Massey, 1985ApJ...291..685A MJ: refers to a recent deep survey for W-R stars by Massey & Johnson, 1996, in preparation N: refers to H II regions with NGC designations. --- CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 22-Oct-96 J_ApJ_469_629.xml An optical and X-ray study of Abell 576, a galaxy cluster with a cold core. J/ApJ/470/724 J/ApJ/470/724 Abell 576 galaxies magnitude and velocities An optical and X-ray study of Abell 576, a galaxy cluster with a cold core. J J Mohr M J Geller D G Fabricant G Wegner J Thorstensen D O Richstone Astrophys. J. 470 724 1996 1996ApJ...470..724M Clusters, galaxy Magnitudes Spectroscopy galaxies: clusters: individual (A576) galaxies: distances and redshifts galaxies: luminosity function, mass function galaxies: photometry X-rays: galaxies We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_<17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_>4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.
Galaxy velocities and photometry RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec R23.5 Isophotal R=23.5mag/arcsec^2^ magnitude mag n_R23.5 Note on R23.5 number=1 #: POSS digitized scan photometry +: Hintzen et al., 1982AJ.....87.1656H *: Marzke & Huchra 1996, in prep. x: Hill et al., 1980ApJ...242L..69H --- e_R23.5 rms uncertainty on R23.5 mag Vel Line-of-sight velocity km/s n_Vel Note on velocity number=1 #: POSS digitized scan photometry +: Hintzen et al., 1982AJ.....87.1656H *: Marzke & Huchra 1996, in prep. x: Hill et al., 1980ApJ...242L..69H --- e_Vel rms uncertainty on Vel km/s Type E: emission; N: non-emission --- James Marcout, Patricia Bauer CDS 1997 Sep 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_470_724.xml Galaxy evolution in Abell 2390. J/ApJ/471/694 J/ApJ/471/694 Abell 2390 Gunn photometry and equivalent widths Galaxy evolution in Abell 2390. R G Abraham T A Smecker-Hane J B Hutchings R G Carlberg H K C Yee E Ellingson S Morris J B Oke M Rigler Astrophys. J. 471 694 1996 1996ApJ...471..694A J/ApJS/102/289 : CNOC cluster redshift survey catalogs. II. (Yee+, 1996) Clusters, galaxy Equivalent widths Galaxies, photometry galaxies: clusters: individual (Abell 2390) galaxies: distances and redshifts galaxies: photometry galaxies: stellar content The galaxy population in the intermediate-redshift (z=0.228) rich cluster Abell 2390 is investigated. We present velocities, colors, and morphological information for an exceptionally large sample of 323 galaxies (216 cluster members) in a 46'x7' (6h^-1^Mpcx1h^-1^Mpc) strip centered on the cD galaxy. This sample of confirmed cluster members is second only to that for the Coma cluster in terms of sample size and spatial coverage in the cluster rest frame and it is the first to trace the transition between a rich cluster and the field at intermediate redshift. The galaxy population in the cluster changes gradually from a very evolved, early-type population in the inner 0.4h^-1^Mpc of the cluster to a progressively later type population in the extensive outer envelope of the cluster from 1 to 3h^-1^Mpc in radius. Radial gradients in galaxy gr color, 4000{AA} break, H{delta} and [O II] line strengths, and morphology are seen in the cluster and are investigated by comparing the data to models computed with the GISSEL spectral synthesis package. The results suggest that the cluster has been built up gradually by the infall of field galaxies over ~8Gyr and that star formation has been truncated in infalling galaxies during the accretion process. The morphological composition of the cluster is shown to be consistent with such a scenario. If true for other clusters, infall-truncated star formation as seen in Abell 2390 may explain both the Butcher-Oemler effect and the large fraction of S0 galaxies in clusters. Only <5% of the galaxies observed in Abell 2390 exhibit evidence for star formation at levels stronger than those seen in typical late-type systems. This suggests that starbursts do not play a major role in driving cluster galaxy evolution at the redshift of Abell 2390, although infall-induced starbursts leading to truncated star formation may have played a role in the earlier history of the cluster. Evidence is found for at least one subcomponent on the west side of the cluster, which is likely to be infalling at the epoch of observation. For a description of the Gunn photometric system, see e.g. <GCPD/38>
ACO 2390 21 53.6 +17 40
Abell 2390 catalog Yee Identification number from Yee et al. (1995ASPC...86..301Y) --- rmag Gunn r-band magnitude mag g-r Gunn g-r color mag e_g-r rms uncertainty on g-r mag Rad Projected radius from central cD arcsec z Redshift --- S/N Signal-to-noise ratio at uniform rest wavelength (see text). --- D4000 4000 Angstroms break 0.1nm e_D4000 rms uncertainty on D4000 0.1nm Hd H{delta} equivalent width 0.1nm e_Hd rms uncertainty on Hd 0.1nm [OII] [O II] {lambda}3727 equivalent width number=1 Only definite 2{sigma} detections are listed. 0.1nm e_[OII] rms uncertainty on [OII] 0.1nm C Morphological index number=2 C is the galaxy's central concentration of light. See Doi et al., 1993MNRAS.264..832D for the complete description of the classification. --- e_C rms uncertainty on C --- mur Limiting isophote of galaxy image mag/arcsec2 Memb Cluster membership classification number=3 field: field galaxy member: cluster member galaxy near: near-field galaxy --- Blue Blueness classification number=4 Blue object are defined to be those galaxies at least 0.25mag bluer in g-r than the color of the red galaxy locus at the projected radius of each individual galaxy. --- James Marcout, Patricia Bauer CDS 1998 Feb 26 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_471_694.xml The Lyman-alpha Forest at z about 4: Keck HIRES Observations of Q0000-26 J/ApJ/472/509 J/ApJ/472/509 Lyman-alpha Forest in Q0000-26 The Lyman-alpha Forest at z about 4: Keck HIRES Observations of Q0000-26 L Lu W L W Sargent D S Womble M Takada-Hidai Astrophy. Jour. 472 509 1996 1996ApJ...472..509L QSOs This file contains the list of absorption lines found in the spectrum of the zem=4.1 quasar Q0000-26 obtained with the 10m Keck I telescope. The spectrum has a resolution of 6.6 km/s, with typical signal-to-noise ratio 25-35 per resolution element. The absorption lines found in the Lyman-alpha forest region has been deblended using the Voigt profile fitting routine VPFIT from Robert Carswell and colleagues; redshift, column density, and Doppler width are provided for each line in the list.
Measured wavelengths No Running number --- lambda Wave length 0.1nm ID Element identification --- z Redshift km/s e_z Mean error of z km/s b Effective radial velocity dispersion km/s e_b Mean error of b km/s logN logN (column density) m-4 e_logN Mean error of logN m-4 n_No Note on observation 1 = This Lyman alpha line is associated with identified metal systems. 2 = This feature agrees with the expected position of S II lambda 1253 in the zabs)=3.39 damped Lyman alpha system. The identification is tentative. 3 = The Si II lambda 1260, and 1304 lines are fitted simultaneously with the Si II lambda 1526 line redward of Lyman alpha emission. 4 = The Fe II lambda 2344 absorption is fitted simultaneously with the Fe II lambda 2586, and 2600 absorption redward of Lyman alpha emission. 5 = The O I lambda 1302 absorption is fitted with the redshift and the Doppler width fixed to those of the corresponding Si II components in the same system, hence there are no error estimates for the redshifts and Doppler widths. One of the components is rejected by VPFIT as not necessary. 6 = The C II lambda 1334 absorption is badly blended with the strong Lyman alpha absorption corresponding to the zabs)=3.8190 C IV system. Only one component of C II is clearly discernible. 7 = Contaminated by cosmic rays or poorly subtracted night sky lines. 8 = This feature has a statistical significance above 3 sigma but less than 4 sigma. 9 = Blended with telluric absorption lines. 10 = The corresponding C IV lambda 1550 absorption occurs in a corrupted part of the spectrum caused by an ink mark on the CCD. --- Redshifts No Running number --- lambda Wave length 0.1nm lam_obs Observed wave length 0.1nm e_lambda Mean error of observed wave length 0.1nm ID Element identification --- z Redshift km/s n_No Note on observation See note on n_No for lu1.dat --- N. G. Roman SSDOO/ADC 1997 Jun 14 J_ApJ_472_509.xml A Minnesota automated plate scanner catalog of galaxies behind the Virgo cluster and toward its antipode J/ApJ/473/822 J/ApJ/473/822 APS Catalog of Galaxies behind Virgo A Minnesota automated plate scanner catalog of galaxies behind the Virgo cluster and toward its antipode G L Hoffman J M Dickey N Y Lu R Fromhold-Treu Astrophys. J. 473 822 1996 1996ApJ...473..822H Galaxies, photometry galaxies: clusters: general galaxies: irregular galaxies: photometry galaxies: spiral Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. <VII/49>) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate. We present a catalog of 1268 galaxies, essentially complete to B<=17.0, found by scanning glass copies of several fields of the original Palomar Sky Survey using the Minnesota Automated Plate Scanner in its isodensitometric mode (as opposed to the threshold densitometric mode used in the APS Catalog of the POSS I). In addition to the different scanning mode, we have employed a different star-galaxy separation method and have visually inspected POSS prints to verify that each image remaining in the catalog is non-stellar. The scanned fields are distributed generally in two areas, one around the outskirts of the Virgo Cluster, the other toward the antipode of the cluster (but still in the northern celestial hemisphere). The catalog gives the position of the center of each galaxy; estimates of the blue and red magnitudes within the outermost threshold crossing and of the blue magnitude extrapolated to zero surface brightness; blue and red diameters of four ellipses fit to the four threshold crossings (approximately 23.8, 23.6, 23.2, and 22.7 mag per square arcsec in blue, and 22.5, 22.4, 21.5 and 21.2 mag per square arcsec in red), and the ellipticities of those four ellipses. The catalog has served as a base from which to draw targets for a Tully-Fisher study of the Virgocentric infall velocity of the Local Group.
Galaxies found by MAPS Field CGCG (Cat. <VII/4>) field number --- No Running index for each field --- Name Name from another catalog --- RAh Right ascension (1950) (hours) h RAm Right ascension (1950) (minutes) min RAs Right ascension (1950) (seconds) s DEd Declination (1950) (degrees) deg DEm Declination (1950) (arcminutes) arcmin DEs Declination (1950) (arcseconds) arcsec B24 B magnitude to lowest threshold number=1 Throughout, B refers to quantities measured on the POSS O plate, R to quantities measured on the POSS E plate. mag Btot B magnitude extrapolated mag diamB1 B diameter to lowest threshold arcsec diamB2 B diameter to second threshold arcsec diamB3 B diameter to third threshold arcsec diamB4 B diameter to highest threshold arcsec eB1 Ellipticity, lowest B threshold --- eB2 Ellipticity, second B threshold --- eB3 Ellipticity, third B threshold --- eB4 Ellipticity, highest B threshold --- R24 R magnitude to lowest threshold number=1 Throughout, B refers to quantities measured on the POSS O plate, R to quantities measured on the POSS E plate. mag diamR1 R diameter to lowest threshold arcsec diamR2 R diameter to second threshold arcsec diamR3 R diameter to third threshold arcsec diamR4 R diameter to highest threshold arcsec eR1 Ellipticity, lowest R threshold --- eR2 Ellipticity, second R threshold --- eR3 Ellipticity, third R threshold --- eR4 Ellipticity, highest Rthreshold --- Patricia Bauer CDS 1997 Feb 11 Lyle Hoffman <hoffmang@nova.phys.lafayette.edu> UNKNOWN UNKNOWN * 14-Apr-1997: Error signaled by Marion Schmitz [NED] (zb4ms@ipac.caltech.edu): Misprint in the field 097, Z979-022 instead of Z097-022. J_ApJ_473_822.xml Colors and K-band counts of extremely faint field galaxies. J/ApJ/475/445 J/ApJ/475/445 VIK photometry of faint field galaxies Colors and K-band counts of extremely faint field galaxies. L A Moustakas M Davis J R Graham J Silk B A Peterson Y Yoshii Astrophys. J. 475 445 1997 1997ApJ...475..445M Galaxies, photometry Photometry, infrared cosmology: observations galaxies: evolution galaxies: photometry galaxies: starburst infrared: galaxies We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I>3; I-K>2, consistent with being early-type galaxies having undergone a burst of star formation at z>5 and viewed at z~1. At K>20, we find several (approximately eight) "red outlier" galaxies with I-K>4 and V-I<2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L<L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.
Object catalog for field I Object catalog for field II RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec xpos X position number=1 North is up, East is left. arcsec ypos Y position number=1 North is up, East is left. arcsec Vmag V magnitude number=2 When the magnitude is '0.0', no reliable value. mag Imag I magnitude number=2 When the magnitude is '0.0', no reliable value. mag Kmag K magnitude mag James Marcout, Patricia Bauer CDS 1997 Oct 24 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_475_445.xml A Composite HST Spectrum of Quasars J/ApJ/475/469 J/ApJ/475/469 Composite HST Spectrum of Quasars A Composite HST Spectrum of Quasars W Zheng G A Kriss R C Telfer J P Grimes A F Davidsen Astrophys. J. 475 469 1997 1997ApJ...475..469Z Photometry, ultraviolet QSOs Redshifts atomic processes quasars: general ultraviolet: galaxies The table data contain the composite spectra from figures 5 and 8 in the printed paper. The table captions are: FIG. 5. Composite FOS spectrum of 101 quasars, binned to 2A. Prominent emission lines and the Lyman limit are labeled, and two possible emission features are marked. The continuum fitting windows are marked with the bars near the bottom. FIG. 8. Composite FOS spectra of 60 radio-loud and 41 radio-quiet quasars, binned to 2A. The flux level in the spectrum for radio-quiet quasars is shifted down for display purposes. We construct a composite quasar spectrum from 284 HST FOS spectra of 101 quasars with redshifts z>0.33. The spectrum covers the wavelengths between 350 and 3000A in the rest frame, with a peak S/N level of ~130 per A at ~1200A. Since ~90% of the sample quasars have redshift z<1.5, the spectrum is suitable for studying the wavelength region shortward of Ly{alpha} without large effects from intervening Ly{alpha} forest absorption. Data in the waveband between 350 and 600A are mainly from the spectra of z>1.5 quasars, for which significant corrections for the accumulated Lyman-series line and continuum absorption have been applied. There is a significant steepening of the continuum slope around 1050A. The continuum between 1050 and 2200A can be modeled as a power law f_{nu} proportional to {nu}_{alpha}_ with {alpha}=-0.99+/-0.05. For the full sample the power-law index in the extreme ultraviolet (EUV) between 350 and 1050A is {alpha}=-1.96+/-0.15. For the radio-loud subsample (60 objects), the EUV spectral index is {alpha}~=-2.2, while for the radio-quiet subsample (41 objects) it is {alpha}~=-1.8. The continuum flux in the wavelengths near the Lyman limit shows a depression of ~10%. The break in the power-law index and the slight depression of the continuum near the Lyman limit are features expected in Comptonized accretion-disk spectra. Comptonization produces a power-law tail in the wavelength band shortward of 1000A and smears out the Lyman-limit edge of the intrinsic accretion-disk spectrum. In the EUV waveband, we detect several possible emission features, including one around 690A that may be O III + N III produced by the Bowen fluorescence effect. Comparing our composite spectrum with one made at higher redshifts by Francis et al. (1991ApJ...373..465F), we find that the equivalent widths of Ly{alpha} and high-ionization emission lines are larger in our sample, reflecting a known luminosity dependence. The equivalent widths of low-ionization lines do not exhibit such a dependence, suggesting that the quasar EUV continuum above ~50eV is steeper at higher luminosity. Radio-quiet quasars appear to show a slightly harder continuum and lower ionization levels in their emission lines.
HST
Composite quasar spectrum Composite spectrum of radio-loud quasars Composite spectrum of radio-quiet quasars Lambda Wavelength 0.1nm Flux Relative F(lambda) --- e_Flux Error in Flux --- RMS RMS deviation per merging spectrum as a fraction of flux --- CDS 1997 Jul 04 AAS CD-ROM series, Volume 8, 1997 Lee E. Brotzman [ADS] 06-May-97 UNKNOWN UNKNOWN Files in the CD-Rom (directory /volume8.apj/v475/p469) are in error. We thank Dr Zheng <zheng@hut4.pha.jhu.edu> for providing the correct files. J_ApJ_475_469.xml The coolest isolated M dwarf and other 2MASS discoveries. J/ApJ/476/311 J/ApJ/476/311 2MASS M-dwarf discoveries The coolest isolated M dwarf and other 2MASS discoveries. J D Kirkpatrick C A Beichman M F Skrutskie Astrophys. J. 476 311K 1997 1997ApJ...476..311K Infrared sources Photometry Stars, dwarfs Stars, late-type infrared: stars stars: late-type stars: low-mass, brown dwarfs surveys We have obtained follow-up spectroscopy of eight late dwarf candidates discovered in a 105deg^2^ area observed with the 2MASS (2 Micron All-Sky Survey) Prototype Camera during test runs between 1992 and 1994. These objects were chosen because of their red infrared colors (e.g., J-Ks>=1.10) and/or red OIR colors (e.g., R-Ks>=6.00). All eight are late M dwarfs, six of which have spectral types later than van Biesbroeck 8 (type M7 V). Despite the fact that we have only followed up a fraction of the reddest sources discovered, the number of known M dwarfs of type M7 and cooler has been increased by 30%. Extrapolation of these results alone shows that over 2000 dwarfs of similar spectral type and with Ks<=14.0 will be imaged by 2MASS over the entire sky. One of these new discoveries is astonishingly cool and has a tentative type of >=M10V. This dwarf, one of the least luminous objects yet discovered, could itself be a high-mass brown dwarf, thus providing another empirical data point in a regime where few such objects are now recognized. Only the substellar suspect GD 165 B and the bona fide brown dwarf GL 229 B, both discovered as companions to known stars, are cooler. Thus, this 2MASS discovery becomes the coolest isolated object so far identified.
Target list of 2MASS discoveries Name 2MASP name number=1 2MASP Jhhmmss[.]s 1 ddmmss; Coordinate designations are in equinox J2000.0, epoch 1993.5. --- l_mu Limit flag on mu --- mu Proper motion number=2 Proper motions were determined by comparing the APM-measured position (epoch ~1950) to the 1993.5-epoch 2MASS position except for 2MASP J0345432+254023, whose measurement is described in Sect. 4.1. The values of {mu} and {theta} in all cases are referred to the J2000.0 equinox. arcsec/yr u_mu Uncertainty flag on mu --- theta Proper motion number=2 Proper motions were determined by comparing the APM-measured position (epoch ~1950) to the 1993.5-epoch 2MASS position except for 2MASP J0345432+254023, whose measurement is described in Sect. 4.1. The values of {mu} and {theta} in all cases are referred to the J2000.0 equinox. deg u_theta Uncertainty flag on theta --- l_RAPM Limit flag on RAPM --- RAPM R_APM_ magnitude number=3 R_APM_: E-plate magnitude. See Irwin et al. (1994, Spectrum 2, 14) for more details. mag Jmag J magnitude mag e_Jmag rms uncertainty on Jmag mag Hmag H magnitude mag e_Hmag rms uncertainty on Hmag mag Ksmag Ks magnitude mag e_Ksmag rms uncertainty on Ksmag mag l_RAPM-Ks Limit flag on RAPM-Ks --- RAPM-Ks RAPM-Ks colour index mag J-Ks J-Ks colour index mag Spectroscopic observations of 2MASS discoveries Name 2MASP name --- SpType Spectral type --- n_SpType Note on SpType number=1 b: Spectral type is tentative pending the discovery of similar low-luminosity objects and the development of quantitative classification criteria for objects of this late type. --- Obs Observation date (UT) "DD/MM/YY" IntTime Integration time s Inst Instrument --- l_Dist Limit flag on Dist --- Dist Estimated distance pc n_Dist Not eon Dist number=2 a: This distance estimate assumes that the object has an age comparable to an average field M dwarf (~1Gyr). If a member of the Pleiades cluster (age~75Myr), it will be more luminous than a field M6.5 dwarf by ~0.8mag at Ks and thus have a distance of ~125pc, consistent with that of the cluster. --- James Marcout, Patricia Bauer CDS 1998 May 05 From ApJ electronic version J_ApJ_476_311.xml New Herbig-Haro flows in L1448 and L1455 J/ApJ/478/603 J/ApJ/478/603 L1448 & L 1455 new Herbig-Haro flows New Herbig-Haro flows in L1448 and L1455 J Bally D Devine V Alten R S Sutherland Astrophys. J. 478 603 1997 1997ApJ...478..603B Radial velocities Stars, pre-main sequence ISM: individual (L1448) ISM: jets and outflows stars: pre-main sequence We present a deep narrowband H{alpha} and [S II] optical survey of a roughly 1deg^2^ region containing L1448 and L1455 in the southwestern region of the Perseus molecular cloud. We report the detection of 13 new groups of Herbig-Haro (HH) objects in this region. The L1448 core contains eight groups of Herbig-Haro objects (HH 193, HH 194, HH 195, HH 196, HH 197, HH 267, HH 268, and HH 277). Many of the new HH objects near L1448 have orientations similar to the L1448C molecular jet and L1448 IRS3 outflow. All four known infrared sources in L1448 power Herbig-Haro objects. L1448 IRS 1 is the likely source of HH 194, HH 195E, and possibly HH 268. L1448 IRS 2 drives HH 195, and L1448 IRS 3 may power HH 196 and possibly HH 193. HH 267 and HH 277 lie close to the axes of the IRS 2 and IRS 3 flows and may also be powered by one of these sources. Finally, the class 0 source L1448C powers HH 197. The L1455 core contains five new groups of HH objects (HH 278, HH 279, HH 280, HH 317, and HH 318). L1455 IRS 1 and L1455 IRS 2 are likely to power HH objects, but a unique association between each IRAS source and a specific HH object is difficult to make. Both clouds contain some HH objects whose driving sources cannot be conclusively identified. Most of the new HH objects are located near the cloud edges while some are in the interclump medium (ICM) more than 1pc from the nearest cloud core or known young stellar object. These observations provide further evidence that HH flows can extend far beyond the cloud cores containing their sources, and in some cases extend over greater distances than associated high-velocity millimeter-wavelength CO emission. Herbig-Haro objects associated with the terminal working surfaces of outflows located in the ICM can be used to probe the nature of the interclump gas in molecular clouds. The large number of HH objects found in relatively inactive star forming regions such as L1448 and L1455 indicates that shock heating and acceleration by protostellar outflows plays an important role in determining the ionization state and energetics of the ICM that surrounds low-mass star forming regions.
L1448 HH objects L1455 HH objects HH HH name --- m_HH Multiplicity index on HH --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) number=1 Coordinates are accurate to within a few arcseconds. s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) number=1 Coordinates are accurate to within a few arcseconds. arcsec SHa H{alpha} flux number=2 Line fluxes are in units of 10^-15ergs/cm^2/s and were calibrated by observations of the standard Feige 34. Fluxes were determined by integrating the emission (summing the counts in each pixel) over the apparent extent of the HH object, then subtracting the background integrated over a nearby region of the same size that was free from HH emission. 10-18W/m2 S[SII] [S II] flux number=2 Line fluxes are in units of 10^-15ergs/cm^2/s and were calibrated by observations of the standard Feige 34. Fluxes were determined by integrating the emission (summing the counts in each pixel) over the apparent extent of the HH object, then subtracting the background integrated over a nearby region of the same size that was free from HH emission. 10-18W/m2 Area Area arcsec+2 RV Radial velocity of the HH object km/s DV Line width of the HH object km/s Source Source name --- James Marcout, Patricia Bauer CDS 1997 Oct 03 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_478_603.xml Planetary nebulae as standard candles. XI. Application to spiral galaxies J/ApJ/479/231 J/ApJ/479/231 PNe in M51, M96 & M101 Planetary nebulae as standard candles. XI. Application to spiral galaxies J J Feldmeier R Ciardullo G H Jacoby Astrophys. J. 479 231 1997 1997ApJ...479..231F J/ApJ/462/1 : PNe in the Coma I region (Jacoby+ 1996) Jacoby, Paper I. 1989ApJ...339...39J Ciardullo et al., Paper II. 1989ApJ...339...53C Jacoby et al., Paper III. 1989ApJ...344..704J Ciardullo et al., Paper IV. 1989ApJ...344..715C Jacoby et al., Paper V. 1990ApJ...356..332J Jacoby et al., Paper VI. 1990ApJ...365..471J Ciardullo et al., Paper VII. 1991ApJ...383..487C Ciardullo et al., Paper VIII. 1992ApJ...388..268C McMillan et al., Paper IX. 1993ApJ...416...62M Jacoby et al., Paper X. 1996ApJ...462....1J, Cat. <J/ApJ/462/1> Planetary nebulae galaxies: distances and redshifts galaxies: individual (M 51, M 96, M 101) galaxies: spiral planetary nebulae: general We report the results of an [O III]{lambda}5007 survey for planetary nebulae (PNs) in three spiral galaxies: M101 (NGC 5457), M51 (NGC 5194/5l95), and M96 (NGC 3368). By comparing on-band/off-band [O III]{lambda}5007 images with images taken in H{alpha} and broadband R. we identify 65, 64, and 74 PN candidates in each galaxy, respectively. From these data, an adopted M31 distance of 770kpc, and the empirical planetary nebula luminosity function (PNLF), we derive distances to M101, M51, and M96 of 7.7+/-0.5, 8.4+/-0.6, and 9.6+/-0.6Mpc. These observations demonstrate that the PNLF technique can be successfully applied to late-type galaxies and can provide an important overlap between the Population I and Population II distance scales. We also discuss some special problems associated with using the PNLF in spiral galaxies, including the effects of dust and the possible presence of [O III] bright supernova remnants.
M101, M51 and M96 planetary nebulae Gal Galaxy name --- PN Planerary number in the galaxy --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Rad Isophotal radius from galaxy arcmin m5007 Lambda5007 magnitude (m5007=-2.5logF5007 - 13.74) mag Note Notes number=1 S: PNe that are part of the statistical samples --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Oct 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_479_231.xml Canada-France Redshift Survey. XIV. Spectral properties of field galaxies up to z=1. J/ApJ/481/49 J/ApJ/481/49 CFRS XIV. Field galaxies up to z=1 Canada-France Redshift Survey. XIV. Spectral properties of field galaxies up to z=1. F Hammer H Flores S J Lilly D Crampton O Le Fevre C Rola G Mallen-Ornelas D Schade L Tresse Astrophys. J. 481 49 1997 1997ApJ...481...49H J/ApJ/455/60 : CFRS II: 0000-00 and 1000+25 fields (Le Fevre+ 1995) J/ApJ/455/75 : CFRS III: 1415+52 and 2215+00 fields (Lilly+ 1995) J/ApJ/455/88 : CFRS IV: 0300+00 field (Hammer+ 1995) J/ApJ/464/79 : CFRS XI: High-redshift field galaxies morphology (Schade+ 1996) J/ApJ/499/112 : HST CFRS and LDSS redshift surveys. I. (Brinchmann+ 1998) Lilly et al. Paper I. 1995ApJ...455...50L Le Fevre et al. Paper II. 1995ApJ...455...60L Lilly et al. Paper III. 1995ApJ...455...75L, Cat. <J/ApJ/455/75> Hammer et al. Paper IV. 1995ApJ...455...88H, Cat. <J/ApJ/455/88> Crampton et al. Paper V. 1995ApJ...455...96C Lilly et al. Paper VI. 1996ApJ...460L...1L Hammer et al. Paper VII. 1995MNRAS.276.1085H Le Fevre et al. Paper VIII. 1996ApJ...461..534L Schade et al. Paper IX. 1996ApJ...464...79S, Cat. <J/ApJ/464/79> Schade et al. Paper X. 1996MNRAS.278...95S Schade D. et al. Paper XI. 1996ApJ...464...79S, Cat. <J/ApJ/464/79> Tresse et al. Paper XII. 1996MNRAS.281..847T Le Fevre et al. Paper XIII. 1996BCFHT..34...10L Galaxies, photometry Galaxies, spectra Redshifts cosmology: observations galaxies: abundances galaxies: evolution galaxies: ISM galaxies: photometry galaxies: stellar content The spectral properties of more than 400 Canada-France Redshift Survey (CFRS) galaxies and their changes over the redshift interval 0<=z<=1.3 are investigated. Emission-line intensities and equivalent widths for accessible lines have been measured, as well as continuum color indices based on 200{AA} wide spectral regions.
Photometry, spectral indices, and emission-line measurements (sample B) CFRS Canada-France Redshift Survey number --- z Redshift --- Kmag K_AB_ magnitude number=1 Magnitude is quoted with the AB normalization scheme (Oke, 1974ApJS...27...21O) mag MB B absolute magnitude mag M1um Absolute magnitude at 1{mu}m mag D3235 UV color index D(3250-3550)(2) --- e_D3235 rms uncertainty on D3235 --- D3538 Balmer index D(3550-3850) number=3 D(3550-3850)=f_nu_(3750-3950)/f_nu_(3450-3650), which is very sensitive to the population of A stars. --- e_D3538 rms uncertainty on D3538 --- D4000 4000{AA} break index number=4 D(4000) as defined by Bruzual (1983ApJ...273..105B), which is the ratio of the average flux density f_nu_ in the bands 4050-4250{AA} and 3750-3950{AA} at rest; this index depends on both metallicity and stellar ages. --- e_D4000 rms uncertainty on D4000 --- D4151 Red color index D(41-50) number=5 D(41-50)=2.5log[f_nu_(4900-5100)/f_nu_(4050-4250)], which follows the definition of Kennicutt (1992ApJ...388..310K) and is rather independent of the hot star population (except for the youngest galaxies), while it varies with metalicity. --- e_D4151 rms uncertainty on D4151 --- Mg2 Mg_2_ index number=6 Mg_2_ index, defined following Faber et al. (1977AJ.....82..941F) and Buzzoni et al. (1992AJ....103.1814B), Mg_2_=-2.5log[f(5156-5197.25)]/[0.39f(4897-4958.25)+0.61f(5303-5366.75)] f standing for f_nu_, where all the flux densities correspond to average values in the corresponding bands, either centered on the Mg feature or at the blue and red sides, respectively: this index depends on both temperature and metallicity (Faber et al., 1977AJ.....82..941F; Faber et al., 1985ApJS...57..711F; Davies et al., 1987ApJS...64..581D) mag e_Mg2 rms uncertainty on Mg2 mag OII O II emission-line intensity number=7 9999: when a line do not appear in the spectral range 9998: when a line was not measurable because of instrumental reasons The intensity unit is the flux density integrated over the emission line F({nu}).d{lambda}, expressed in 10-29 erg.s-1.Hz-1.cm-2*{AA} = erg.{AA}.cm-2 10-33nm.W/m2/Hz e_OII rms uncertainty on OII 10-33nm.W/m2/Hz W(OII) O II equivalent width number=7 9999: when a line do not appear in the spectral range 9998: when a line was not measurable because of instrumental reasons The intensity unit is the flux density integrated over the emission line F({nu}).d{lambda}, expressed in 10-29 erg.s-1.Hz-1.cm-2*{AA} = erg.{AA}.cm-2 0.1nm e_W(OII) rms uncertainty on W(OII) 0.1nm OIII O III emission-line intensity number=7 9999: when a line do not appear in the spectral range 9998: when a line was not measurable because of instrumental reasons The intensity unit is the flux density integrated over the emission line F({nu}).d{lambda}, expressed in 10-29 erg.s-1.Hz-1.cm-2*{AA} = erg.{AA}.cm-2 10-33nm.W/m2/Hz e_OIII rms uncertainty on OIII 10-33nm.W/m2/Hz W(OIII) O III equivalent width number=7 9999: when a line do not appear in the spectral range 9998: when a line was not measurable because of instrumental reasons The intensity unit is the flux density integrated over the emission line F({nu}).d{lambda}, expressed in 10-29 erg.s-1.Hz-1.cm-2*{AA} = erg.{AA}.cm-2 0.1nm e_W(OIII) rms uncertainty on W(OIII) 0.1nm W(Hbeta) Hbeta equivalent width number=7 9999: when a line do not appear in the spectral range 9998: when a line was not measurable because of instrumental reasons The intensity unit is the flux density integrated over the emission line F({nu}).d{lambda}, expressed in 10-29 erg.s-1.Hz-1.cm-2*{AA} = erg.{AA}.cm-2 0.1nm e_W(Hbeta) rms uncertainty on W(Hbeta) 0.1nm W(Halpha) Halpha equivalent width number=7 9999: when a line do not appear in the spectral range 9998: when a line was not measurable because of instrumental reasons The intensity unit is the flux density integrated over the emission line F({nu}).d{lambda}, expressed in 10-29 erg.s-1.Hz-1.cm-2*{AA} = erg.{AA}.cm-2 0.1nm e_W(Halpha) rms uncertainty on W(Halpha) 0.1nm James Marcout, Patricia Bauer CDS 1998 Aug 13 UNKNOWN UNKNOWN From ApJ electronic version J_ApJ_481_49.xml The identification of EGRET sources with flat-spectrum radio sources. J/ApJ/481/95 J/ApJ/481/95 Radio identification of EGRET sources The identification of EGRET sources with flat-spectrum radio sources. J R Mattox J Schachter L Molnar R C Hartman A R Patnaik Astrophys. J. 481 95 1997 1997ApJ...481...95M J/ApJS/101/259 : The second EGRET catalog (Thompson+ 1995) J/ApJS/107/227 : Supplement to Second EGRET Catalog (Thompson+ 1996) Fichtel et al., The first EGRET catalog 1994ApJ....94..551F Active gal. nuclei Cross identifications Gamma rays Radio sources galaxies: active gamma rays: observations quasars: general We present a method to assess the reliability of the identification of EGRET sources with extragalactic radio sources. We verify that EGRET is detecting the blazar class of active galactic nuclei (AGNs). However many published identifications are found to be questionable. We provide a table of 42 blazars that we expect to be robust identifications of EGRET sources. This includes one previously unidentified EGRET source, the lensed AGN PKS 1830-210, near the direction of the Galactic center. We provide the best available positions for 16 more radio sources that are also potential identifications for previously unidentified EGRET sources. All high Galactic latitude EGRET sources (|b|>3) that demonstrate significant variability can be identified with flat-spectrum radio sources. This suggests that EGRET is not detecting any type of AGN other than blazars. This identification method has been used to establish with 99.998% confidence that the peak gamma-ray flux of a blazar is correlated with its average 5GHz radio flux. An even better correlation is seen between gamma-ray flux and the 2.29GHz flux density measured with VLBI at the base of the radio jet. Also, using high-confidence identifications, we find that the radio sources identified with EGRET sources have greater correlated VLBI flux densities than the parent population of flat radio spectrum sources.
CGRO
Potential radio identifications of sources in the second EGRET catalog Potential radio identifications of EGRET sources in the supplement to the second EGRET catalog 2EG J2000 position name of the EGRET source --- n_2EG Note number=1 c: Verbunt et al. (1996A&A...311L...9V) identify this source with millisecond pulsar J0218+4232. f: Identification analysis not performed, radio survey source confused j: Not (completely) in GB or PMN survey. --- GLON Galactic longitude deg GLAT Galactic latitude deg n_GLAT Note on GLAT number=2 k: Using the position of Hunter et al. (1994ApJ...436..216H), which differs significantly from that of Thompson et al. (1995, Cat. <J/ApJS/101/259>) because of the use of a different Galactic diffuse model. m: Position estimate (and error ellipse a=35', b=20', {phi}=8{deg}) obtained from VP7.2 with E>1000Mev data, the analysis used for the identification of Thompson et al. (1995, Cat. <J/ApJS/101/259>) with 2022-077. --- VI Variability index number=3 Variability index, -logP, where P is the probability that the source is invariant based on a {chi}^2^ test of flux for all available viewing periods. A grater variability index corresponds to a higher probability that the source is variable --- ID EGRET catalogue identification (OtherName in EGRET catalog description) --- u_ID ?: lower confidence level, else high-confidence level --- RadioID Possible radio counterpart number=4 B1950 position are used for Green Bank sources and original J2000 position names are used for PMN sources --- n_RadioID Note number=5 a: Planetary nebula. b: Shows OVV behavior. d: A gamma-ray hare was reported by Lundgren et al. (1995IAUC.6258....1L) during the 1995 August 8-22 EGRET exposure. An optical spectrum (S. Lundgren 1997, private communication) found only a BL Lac-type continuum spectrum. g: This potential identification indicated by Mukherjee et al. (1995ApJ...445..189M) and Nolan et al. (1996ApJ...459..100N). i: Dingus et al. (1996ApJ...467..589D) note this possible identification. n: Fich (1993ApJS...86..475F) identified this extended radio source with an H II region. Therefore, it is unlikely to be the EGRET source. x: A {gamma}-flare of this source (NRAO 190) was observed by McGlynn et al., 1997ApJ...481..625M y: This potential identification noted by Thompson et al. (1996ApJS..107..227T , their table2) --- Names Other name of counterpart ---- n_Names Note number=6 e: Classified as a galaxy by Stickel & Kuhr 1994. However, S. Wagner (1996, private communication) finds optical variability on a ~ 1week timescale. h: This source is very likely to be the EGRET source because it is detected at TeV energies (Buckley et al., 1996ApJ...472L...9B). l: Classified as a galaxy by Stickel & Kuhr (1994, Cat. <J/A+AS/105/211>) w: 0219+428 = 3C 66 --- S5GHz Density flux at 4.85GHz mJy SI Radio spectral index --- r0 Characteristic angle between confusing sources that are at least as bright and flat as this radio source arcmin eta a priori probability {eta} = p(id) that the source is a {gamma}-ray source --- r Angle between the EGRET position estimate and the radio position arcmin r95 Radius of the 95% confidence contour in the direction of the radio source arcmin Contour Position contour at the radio position % LR Likelihood ratio indicating the strength of the indication for the determination --- p(id/r) a posteriori probability that the identification is correct --- James Marcout, Patricia Bauer CDS 1997 Oct 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_481_95.xml The surface brightness fluctuations and globular cluster population of NGC 4478. J/ApJ/483/745 J/ApJ/483/745 NGC 4478 globular clusters The surface brightness fluctuations and globular cluster population of NGC 4478. E H Neilsen Z I Tsvetanov H C Ford Astrophys. J. 483 745 1997 1997ApJ...483..745N Clusters, globular Photometry galaxies: distances and redshifts galaxies: individual (NGC 4478) galaxies: star clusters We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre & Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.
Globular cluster candidate catalog NTF97 Sequential number --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Vmag V magnitude mag V-I V-I colour index mag James Marcout, Patricia Bauer CDS 1998 May 12 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJ_483_745.xml Berkeley 17: the oldest open cluster? J/ApJ/483/826 J/ApJ/483/826 BVI CCD photometry of Berkeley 17 Berkeley 17: the oldest open cluster? R L Phelps Astrophys. J. 483 826 1997 1997ApJ...483..826P Clusters, open Photometry, CCD Hertzsprung-Russell (HR diagram) open clusters and associations: individual (Berkeley 17) stars: abundances stars: evolution Faint magnitude BVI CCD photometry of the central region of the old open cluster Berkeley 17 (Be 17) has been undertaken to investigate the claim that it is the oldest open cluster yet discovered (Phelps, Janes, & Montgomery, 1994AJ....107.1079P). This study reveals Be 17 to have a metallicity -0.30<=[Fe/H]<=0.00; a reddening 0.52<=E(B-V)<=0.68 or 0.61<=E(V-I)<=0.71; a distance modulus, (m-M)_0_=12.15+/-0.10, corresponding to a distance of 2.7+/-0.1kpc; a diameter of ~10pc; a minimum mass of 400 Msun; and an age of 10-13Gyr. With an adopted age of 12(+1)(-2)Gyr, these results suggest that Be 17 is indeed the oldest open cluster yet discovered. The inferred old age for Be 17 indicates that the cluster is an important one for studies of the differences between open and globular clusters, the transition from the halo/thick disk to the thin disk of the Galaxy, and even for establishing the minimum age of the universe.
Cl Berkeley 17 C 0517+305 05 20.6 +30 36
V, B-V color-magnitude diagram data for Be 17 ID Identification number --- Xpos X coordinate number=1 1 pix = 0.30". pix Ypos Y coordinate number=1 1 pix = 0.30". pix Vmag V magnitude mag B-V B-V color mag e_Vmag Error in Vmag mag e_B-V Error in B-V mag V, V-I color-magnitude diagram data for Be 17 V, V-I color magnitude diagram data for the Be 17 off-cluster control field ID Identification number --- Xpos X coordinate number=1 1 pix = 0.30". pix Ypos Y coordinate number=1 1 pix = 0.30". pix Vmag V magnitude mag V-I V-I color mag e_Vmag Error in Vmag mag e_V-I Error in V-I mag UNKNOWN 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee E. Brotzman [ADS] 24-Jul-97 J_ApJ_483_826.xml New Perspectives on AX Monocerotis J/ApJ/484/394 J/ApJ/484/394 AX Mon photometry and UV spectra New Perspectives on AX Monocerotis N M Elias II R E Wilson E C Olson J P Aufdenberg E F Guinan M Guedel W V Van Hamme H L Stevens Astrophys. J. 484 394 1997 1997ApJ...484..394E Binaries, spectroscopic Photometry, UBV Photometry, uvby Radial velocities Spectra, ultraviolet binaries: spectroscopic circumstellar matter radio continuum: stars stars: emission-line, Be stars: individual (AX Mon) ultraviolet: stars AX Monocerotis is a 232d, noneclipsing, interacting binary star that consists of a K giant, a Be-like giant, and a large amounts of circumstellar material. The K star is almost certainly a synchronous rotator and is probably in contact with its critical lobe. The Be star was believed to be a rapid rotator based on extremely wide absorption lines, but new spectra show that these lines arise from the circumstellar environment. Hydrogen emission, also circumstellar, is many times stronger than the continuum. Near-ultraviolet light curves exhibit a 0.5 mag dip near phase 0.75, but there is no such variability at longer wavelengths. Gas flow trajectories from the cusp of the K star toward the Be star provide a simple explanation for the photometric and spectroscopic behavior. We may have found a decreasing orbital period, but more data are necessary to confirm this result. We present several models for AX Mon based on (1) new and archival visible photometry, (2) archival ultraviolet spectroscopy, (3) new and archival visible spectroscopy, (4) new visible polarimetry, and (5) new radio photometry. Further observations, including optical interferometry, are proposed.
AX Mon 06 30 32.9 +05 52 00 HD 46966 06 36 25.8 +06 04 59
H{alpha}, uvby and UBV photometry Band Photometric band number=1 hn: H{alpha} narrow photometry hw: H{alpha} wide photometry u: Stromgren u photometry b: Stromgren b photometry v: Stromgren v photometry y: Stromgren y photometry U: Johnson U photometry B: Johnson B photometry V: Johnson V photometry --- HJD Heliocentric Julian Date d dMag Magnitude difference number=2 Magnitude difference in the sense variable minus comparison. The comparison star was HD 46966 (BD +06 1301). mag Blue, green and red polarimetry Band Polarimetry band number=1 b: blue g: green r: red --- HJD Heliocentric Julian Date d q Stokes q value number=2 q = P_l_cos2{theta} and u=P_l_in2{theta} where P_l_ is the linear polarisation and {theta} the linear polarisation electric vector --- e_q Error in q --- u Stokes u value number=2 q = P_l_cos2{theta} and u=P_l_in2{theta} where P_l_ is the linear polarisation and {theta} the linear polarisation electric vector --- e_u Error in u --- v Stokes v value --- e_v Error in v --- Star 2 (hot component of AX Mon) radial velocities HJD Heliocentric Julian Date d vsini Star 2 radial velocity km/s RW Relative weight number=1 For Cowley and Mastenova, the weights are based on the variances of the individual data sets, and for the authors' data they are based on the cross-correlation fit variances. --- Obs Observer number=2 1 = Cowley A.P., 1964ApJ...139..817C 2 = Mastenova K., 1989BAICz..40..118M 3 = Aufdenberg J.P., this work --- Spec. (638-672 nm), 1993/12/28, ECO Spec. (439-456 nm), 1994/01/01, ECO Spec. (769-796 nm), 1994/01/01, ECO Spec. (577-610 nm), 1994/01/03, ECO Spec. (541-548 nm), 1993/11/18, JPA Spec. (555-561 nm), 1993/11/18, JPA Spec. (569-576 nm), 1993/11/18, JPA Spec. (584-591 nm), 1993/11/18, JPA Spec. (600-607 nm), 1993/11/18, JPA Spec. (616-623 nm), 1993/11/18, JPA Spec. (634-641 nm), 1993/11/18, JPA Spec. (653-660 nm), 1993/11/18, JPA Spec. (673-680 nm), 1993/11/18, JPA Spec. (541-548 nm), 1993/12/01, JPA Spec. (555-561 nm), 1993/12/01, JPA Spec. (569-576 nm), 1993/12/01, JPA Spec. (584-591 nm), 1993/12/01, JPA Spec. (600-607 nm), 1993/12/01, JPA Spec. (616-623 nm), 1993/12/01, JPA Spec. (634-641 nm), 1993/12/01, JPA Spec. (653-660 nm), 1993/12/01, JPA Spec. (673-680 nm), 1993/12/01, JPA Spec. (541-548 nm), 1993/02/27, JPA Spec. (555-561 nm), 1993/02/27, JPA Spec. (569-576 nm), 1993/02/27, JPA Spec. (584-591 nm), 1993/02/27, JPA Spec. (600-607 nm), 1993/02/27, JPA Spec. (616-623 nm), 1993/02/27, JPA Spec. (634-641 nm), 1993/02/27, JPA Spec. (653-660 nm), 1993/02/27, JPA Spec. (673-680 nm), 1993/02/27, JPA Date Observation date "DD/MM/YY" Lambda Wavelength nm Flux Flux normalized to estimated continuum --- Patricia Bauer CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee E. Brotzman [ADS] 24-Jul-97 J_ApJ_484_394.xml All-Sky 4.85 GHz flux measurements of H II regions J/ApJ/488/224 J/ApJ/488/224 4.85 GHz fluxes of H II regions All-Sky 4.85 GHz flux measurements of H II regions T A Kuchar F O Clark Astrophys. J. 488 224 1997 1997ApJ...488..224K VIII/38 : The Parkes-MIT-NRAO 4.85GHz (PMN) Surveys (Griffith+ 1993-1996) VIII/14 : 87GB Catalog of radio sources (Gregory et al., 1991) H II regions Radio sources Surveys HII regions radio continuum: ISM surveys We present an all-sky flux catalog of 760 H II regions with angular sizes ranging up to 10' at 4.85GHz. The data were compiled in a self-consistent manner from existing images of the Green Bank and Parkes-MIT-NRAO 4.85GHz radio continuum surveys. Nearly 35% of these H II regions have fluxes measured from these surveys for the first time. We compared our results to the previously published source catalogs which fit the same data. The new flux measurements agree within 5%-7% of these values and fall well within the formal errors. The diameters fall within 16% of the previously published fits to the same data, within the formal uncertainties of these values.
87GB (Cat. <VIII/14>) source list PMN (Cat. <VIII/38>) source list Name Source name in format Glll.l+/-bb.b --- GLON Galactic longitude deg GLAT Galactic latitude deg VLSR LSR Velocity (if known) km/s RAh Right Ascension (1950) h RAm Right Ascension (1950) min RAs Right Ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Flux 4.85 GHz peak flux density (mJy/beam) mJy Diam FWHM of source (convolved w/telescope beam) arcmin Refs HII Region Survey References 1 - Lockman, 1989ApJS...71..469L 2 - Reifenstein et al., 1970A&A.....4..357R 3 - Downes et al., 1980A&AS...40..379D 4 - Fich & Blitz, 1984ApJ...279..125F 5 - Wilson et al., 1970A&A.....6..364W 6 - Caswell & Haynes, 1987A&A...171..261C --- Notes Source Comments A = Additional recombination line at this position T = Saturation of the telescope analog-to-digital converters M = Multiple measurement of source C = Complex field S = Stronger source nearby X = very strong (>10Jy) source nearby --- CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee E. Brotzman [ADS] 29-Jul-97 J_ApJ_488_224.xml The "mass discrepancy" for massive stars: tests of models using spectroscopic binaries J/ApJ/490/328 J/ApJ/490/328 "Mass Discrepancy" for Massive Stars The "mass discrepancy" for massive stars: tests of models using spectroscopic binaries V Burkholder P Massey N Morrell Astrophys. J. 490 328 1997 1997ApJ...490..328B Binaries, spectroscopic Radial velocities binaries: spectroscopic stars: early-type stars: evolution stars: fundamental parameters Stellar evolutionary models are often used to infer a star's mass via its luminosity, but empirical checks on the accuracy of the theoretical mass-luminosity relation for very massive stars have been lacking. This is of particular concern given that modern atmosphere models yield systematically smaller masses for massive stars than do evolutionary models, with the discrepancy a factor of two for Of stars. We attempt to resolve this mass discrepancy by obtaining new, high-resolution optical data on seven early-type spectroscopic binaries: V453 Cyg, HD 191201, V382 Cyg, Y Cyg, HD 206267, DH Cep, and AH Cep. Our study produces improved spectral subtypes for the components of these systems, crucial for evaluating their luminosities and locations in the H-R diagram. Our radial velocity study utilizes a measuring method which explicitly accounts for the effects of pair-blending. We combine our new orbit solutions with existing data on inclinations and distances when available to compare the orbital masses with evolutionary models, and we find good agreement in all cases where the stars are non-interacting. (The components of V382 Cyg and DH Cep fill their Roche lobes, and in both cases we find masses substantially lower than the masses inferred from evolutionary tracks, suggesting that significant material has been lost rather than transferred. We confirm that this same trend exists for other systems drawn from the literature.) Our own data extends to only 15 M_{sun}_, although photometric inclination determinations for HD 191201 and HD 206267 should prove possible, and will provide examples of higher mass systems. We briefly discuss suitable systems from the literature, and conclude that orbit solutions provide good agreement with the evolutionary models to 25 M_{sun}_. Beyond this, most known binaries either fill their Roche lobes or have other complications. We also discuss five systems for which our improved data and analysis failed to yield acceptable orbit solutions: EO Aur, IU Aur, V640 Mon (Plaskett's star), LY Aur, and 29 UW CMa all remained intractable, despite improved data.
AH Cep HD 216014 22 47 53.0 +65 03 44 DH Cep HD 215835 22 46 54.1 +58 05 03 HD 191201 20 07 23.7 +35 43 06 HD 206267 21 38 57.5 +57 29 21 V382 Cyg HD 228854 20 18 47.2 +36 20 27 V453 Cyg HD 227696 20 06 34.9 +35 44 27 Y Cyg HD 198846 20 52 03.5 +34 39 29
Radial velocities ID Star identification --- HJD Heliocentric Julian Date d Phase Orbital phase --- RVp Radial velocity of the primary, RV(p) km/s O-Cp Obs. RV(p) minus calculated orbital velocity km/s WTp Weight given RV(p) in computing orbit The weight given the primary's, or secondary's, radial velocity in computing the orbit, usually sqrt(number of lines measured). --- RVs Radial velocity of the secondary, RV(s) km/s O-Cs Obs. RV(s) minus calculated orbital velocity km/s WTs Weight given RV(s) in computing orbit --- CDS 1998 Feb 05 AAS CD-ROM series, Volume 9, 1997 Lee E. Brotzman [ADS] 27-Jul-97 J_ApJ_490_328.xml A major star formation region in the receding tip of the stellar Galactic bar J/ApJ/491/L31 J/ApJ/491/L31 TMGS star positions A major star formation region in the receding tip of the stellar Galactic bar F Garzon M Lopez-Corredoira P Hammersley T J Mahoney X Calbet J E Beckman Astrophys. J. 491, L31 ??? ??? 1997 1997ApJ...491L..31G Galactic plane Positional data Galaxy: stellar content Galaxy: structure stars: formation We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.
Coordinates of the TMGS sample RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Class S: supergiant; blank: giant --- table1.tex LaTeX version of table1 Patricia Bauer CDS 1998 Jan 30 Martin Lopez-Corredoira <martinlc@ll.iac.es> J_ApJ_491_L31.xml The properties of poor groups of galaxies. I. Spectroscopic survey and results. J/ApJ/496/39 J/ApJ/496/39 Properties of poor groups of galaxies. I. The properties of poor groups of galaxies. I. Spectroscopic survey and results. A I Zabludoff J S Mulchaey Astrophys. J. 496 39 1998 1998ApJ...496...39Z Clusters, galaxy Radial velocities galaxies: clusters: general galaxies: distances and redshifts galaxies: elliptical and lenticular, cD galaxies: evolution galaxies: interactions large-scale structure of universe X-rays: galaxies We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).
Galaxy data Name Galaxy name --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec HRV Heliocentric radial velocity number=1 The velocities are either emission-line velocities, absorption-line velocities, or a weighted average of the two km/s e_HRV rms uncertainty on HRV km/s Line Type of measurement number=2 0: absorption lines 1: emission lines 2: combination of both --- MType Morphological type number=3 E: early type S: late type --- Plate Plate/CCD number=4 p: plate c: CCD --- r_HRV Heliocentric radial velocity reference number=5 N: from NED --- Group kinematic properties Group Group name --- RAh Right ascension of the group optical projected centroid in J2000 h RAm Right ascension of the group optical projected centroid in J2000 min RAs Right ascension of the group optical projected centroid in J2000 s DE- Declination sign --- DEd Declination of the group optical projected centroid in J2000 deg DEm Declination of the group optical projected centroid in J2000 arcmin DEs Declination of the group optical projected centroid in J2000 arcsec Ntot Total number of galaxies with measured redshifts in the fiber field --- Ngroup Number of group members --- HRV Biweight estimators of the mean heliocentric velocity km/s e_HRV rms uncertainty on HRV km/s sigma Line-of-sight velocity dispersion km/s E_sigma Error on sigma (upper limit) km/s e_sigma Error on sigma (lower limit) km/s rsample Physical radius of the group sampled by the fiber field (h^-1^Mpc) Mpc rp Pair radius (h^-1^Mpc) Mpc rh Mean harmonic (virial )radius (h^-1^Mpc) Mpc Mvir Virial mass (h^-1^Mpc) solMass tc/tH Ratio of the crossing time to Hubble time --- James Marcout, Patricia Bauer CDS 1998 Jun 15 UNKNOWN UNKNOWN From ApJ electronic version J_ApJ_496_39.xml Morphological studies of the galaxy populations in distant "Butcher-Oemler" clusters with the Hubble Space Telescope. II. AC 103, AC 118, and AC 114 at z = 0.31. J/ApJ/497/188 J/ApJ/497/188 A103, A118 and A114 morphological studies Morphological studies of the galaxy populations in distant "Butcher-Oemler" clusters with the Hubble Space Telescope. II. AC 103, AC 118, and AC 114 at z = 0.31. W J Couch A J Barger I Smail R S Ellis R M Sharples Astrophys. J. 497 188 1998 1998ApJ...497..188C Clusters, galaxy Equivalent widths Morphology Photometry galaxies: clusters: individual (AC 103, AC 114, AC 118) galaxies: evolution galaxies: interactions galaxies: structure We present the results of a program to study the detailed morphologies of galaxies in intermediate-redshift clusters and hence understand the physical origin of the enhanced star formation seen in the environments at earlier epochs. Deep, high-resolution imagery has been obtained of three rich clusters, AC 103, AC 118 and AC 114 at z=0.31, through the R (F702W) filter of the Wide Field Planetary Camera (WFPC2) of the Hubble Space Telescope (HST).
HST
New spectroscopic results Cluster Cluster name --- Tel Telescope number=1 AAT: Anglo-Austalian Telescope NTT: New Technology Telescope --- Inst Instrument number=2 LDSS-1: Low Dispersion Survey Spectrograph on AAT EMMI: European Multi-Mode Imager/Spectrograph on NTT --- HST HST number number=3 Identity number of each object in SExtractor catalog derived from our WFPC2 images. The absence of entry indicates that the object lies outside the WFPC2 field. --- CN84 Couch & Newell (1984ApJS...56..143C) number --- m_CN84 Multiplicity index on CN84 --- BAE96 Barger et al. (1996MNRAS.279....1B) number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Rmag R magnitude mag K'mag K' magnitude mag B-R B-R (or U-i if n_B-R=a) colour index mag n_B-R a: U-I colour index from BAE96 in B-R column --- z Redshift --- u_z Uncertainty flag on z number=4 The presence of a colon denotes that the measurement is based on just one line emission, assumed in all cases to be [O II] {lambda}3727. --- EW(3727) Equivalent width of [O II] {lambda}3727 emission line 0.1nm e_EW(3727) rms uncertainty on EW(3727) 0.1nm EW(Hd) Equivalent width of H{delta} absorption line 0.1nm e_EW(Hd) rms uncertainty on EW(Hd) 0.1nm SpType Spectral type number=5 Psv(pec): galaxies whose spectra have all the same characteristics as the passive types but whose colors are marginally bluer. --- Morphological classifications for AC 103, AC 118, and AC 114 Cluster Cluster name --- HST HST number --- CN84 Couch & Newell (1984ApJS...56..143C) number --- m_CN84 Multiplicity index on CN84 --- xpos X coordinate from HST pix ypos Y coordinate from HST pix R702 R (F702W filter) magnitude mag Mtype Hubble type --- MDS Classifications on the numerical scheme devised by Glazebrook et al. (1995MNRAS.275...19G) number=1 0= E 1= E/S0 2= S0 3= Sa-Sb 4= S 5= Sc-Sdm 6= Irr 7= unclassified object 8= galaxy merger -1= same "compact" morphology as found here --- Status Int/Merg/Sat number=2 I or i: interactive M or m: merger T or t: tidal evidence Sat: galaxies with faint satellites --- Com Comments --- James Marcout, Patricia Bauer CDS 1998 Jun 22 UNKNOWN UNKNOWN From the ApJ electronic version J_ApJ_497_188.xml Candidate main-sequence stars with debris disks: a new sample of Vega-like sources. J/ApJ/497/330 J/ApJ/497/330 Candidate main-sequence stars Candidate main-sequence stars with debris disks: a new sample of Vega-like sources. V Mannings M J Barlow Astrophys. J. 497 330 1998 1998ApJ...497..330M II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989) III/31 : Michigan catalogue for the HD stars, vol. 1 (Houk+, 1975) III/51 : Michigan Catalogue of HD stars, Vol.2 (Houk, 1978) III/80 : Michigan Catalogue of HD stars, Vol.3 (Houk, 1982) III/133 : Michigan Catalogue of HD stars, Vol.4 (Houk+, 1988) Infrared sources Spectra, infrared Stars, dwarfs circumstellar matter infrared: stars Vega-like sources are main-sequence stars that exhibit IR fluxes in excess of expectations for stellar photospheres, most likely due to reradiation of stellar emission intercepted by orbiting dust grains. We have identified a large sample of main-sequence stars with possible excess IR radiation by cross-correlating the Michigan Catalog of Two-dimensional Spectral Types for the HD Stars with the IRAS Faint Source Survey Catalog. Some 60 of these Vega-like sources were not found during previous surveys of the IRAS database, the majority of which employed the lower sensitivity Point Source Catalog. Here, we provide details of our search strategy, together with a preliminary examination of the full sample of Vega-like sources.
Newly identified candidate main-sequence stars with debris disks Michigan Spectral Catalogue Vega-like stars identified with in our search and in previous studies Vega-like candidates with uncertain luminosity classification Classical Be stars extracted during our search for Vega-like sources Number Object number --- n_Number Note on Number number=1 a: Flagged by SIMBAD as a double or multiple star b: Flagged by SIMBAD as a variable star c: Has a K4 companion star (Corbally, 1984ApJS...55..657C) e: Member of stellar cluster f: {lambda} Boo star (e.g., King, 1994MNRAS.269..209K) g: Classed as Herbig Ae star by Finkenzeller & Mundt (1984A&AS...55..109F) h: Located in R CrA star-forming region i: Member of Sco-Cen OB association (e.g., de Geus, de Zeeuw, & Lub, 1989A&A...216...44D) j: Not identified in previous surveys of the IRAS database --- HD HD (Cat. <III/135>) number --- SAO SAO (Cat. <I/131>) number --- HR HR (Cat. <V/50>) number --- Name Object name --- SpType Spectral type --- Fqual Quality flag of the IRAS bands --- F12um FSC (Cat. <II/156>) flux density at 12{mu}m Jy e_F12um rms uncertainty on F12um Jy F25um FSC (Cat. <II/156>) flux density at 25{mu}mm Jy e_F25um rms uncertainty on F25um Jy F60um FSC (Cat. <II/156>) flux density at 60{mu}mm Jy e_F60um rms uncertainty on F60um Jy F100um FSC (Cat. <II/156>) flux density at 100{mu}mm Jy e_F100um rms uncertainty on F100um Jy D(12/25)/dobs Discrepancy for 12{mu}m/25{mu}m ratio number=2 Measure of the significance of the discrepancies between the observed flux density ratios and the expected photospheric values, as defined in eqs. (5) and (6). A null entry signifies inadequate data quality --- D(25/60)/dobs Discrepancy for 25{mu}m/60{mu}m ratio number=2 Measure of the significance of the discrepancies between the observed flux density ratios and the expected photospheric values, as defined in eqs. (5) and (6). A null entry signifies inadequate data quality --- James Marcout, Patricia Bauer CDS 1998 Jun 16 UNKNOWN UNKNOWN From ApJ electronic version J_ApJ_497_330.xml A spectroscopic survey of the galaxy cluster CL 1358+62 at z = 0.328. J/ApJ/498/195 J/ApJ/498/195 Spectroscopic survey of CL 1358+62 A spectroscopic survey of the galaxy cluster CL 1358+62 at z = 0.328. D Fisher D Fabricant M Franx P Van Dokkum Astrophys. J. 498 195 1998 1998ApJ...498..195F J/ApJ/500/714 : Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998) Clusters, galaxy Photometry Redshifts Spectroscopy galaxies: clusters: individual (CL 1358+6345) galaxies: distances and redshifts galaxies: evolution galaxies: kinematics and dynamics galaxies: structure We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.
ClG 1358+62 ZwCl 1358+6245 13 59 54.0 +62 30 36
CL 1358+62 catalog [FFF98] Identification number ([FFF98] NNNN) --- xpos x position number=1 Positions are given with respect to the brightest cluster galaxy (number 375) at RA=13h58m20.7s, DE=+62{deg}45'33" (1950), with positive x to the west and positive y to the north. arcsec ypos y position number=1 Positions are given with respect to the brightest cluster galaxy (number 375) at RA=13h58m20.7s, DE=+62{deg}45'33" (1950), with positive x to the west and positive y to the north. arcsec Rmag R magnitude mag V-R V-R colour index mag z Redshift --- e_z rms uncertainty on z --- Hd Line strength index H{delta} number=2 The strength of each spectral index is a measure of the flux in the central bandpass compared to a continuum level set by the sidebands. ------------------------------------------------------------------ Line strength index definitions: ------------------------------------------------------------------ Index Bandpass Blue Sideband Red Sideband ------------------------------------------------------------------ Hdelta 4083.500-4122.250 4017.00-4057.00 4153.00-4193.00 Hgamma 4319.750-4363.500 4242.00-4282.00 4404.00-4444.00 Hbeta 4847.875-4876.625 4799.00-4839.00 4886.00-4926.00 [O II] 3716.300-3738.300 3696.30-3716.30 3738.30-3758.30 --- e_Hd rms uncertainty on Hd --- Hg Line strength index H{gamma} number=2 The strength of each spectral index is a measure of the flux in the central bandpass compared to a continuum level set by the sidebands. ------------------------------------------------------------------ Line strength index definitions: ------------------------------------------------------------------ Index Bandpass Blue Sideband Red Sideband ------------------------------------------------------------------ Hdelta 4083.500-4122.250 4017.00-4057.00 4153.00-4193.00 Hgamma 4319.750-4363.500 4242.00-4282.00 4404.00-4444.00 Hbeta 4847.875-4876.625 4799.00-4839.00 4886.00-4926.00 [O II] 3716.300-3738.300 3696.30-3716.30 3738.30-3758.30 --- e_Hg rms uncertainty on Hg --- Hb Line strength index H{beta} number=2 The strength of each spectral index is a measure of the flux in the central bandpass compared to a continuum level set by the sidebands. ------------------------------------------------------------------ Line strength index definitions: ------------------------------------------------------------------ Index Bandpass Blue Sideband Red Sideband ------------------------------------------------------------------ Hdelta 4083.500-4122.250 4017.00-4057.00 4153.00-4193.00 Hgamma 4319.750-4363.500 4242.00-4282.00 4404.00-4444.00 Hbeta 4847.875-4876.625 4799.00-4839.00 4886.00-4926.00 [O II] 3716.300-3738.300 3696.30-3716.30 3738.30-3758.30 --- e_Hb rms uncertainty on Hb --- [OII] Line strength index [O II] number=2 The strength of each spectral index is a measure of the flux in the central bandpass compared to a continuum level set by the sidebands. ------------------------------------------------------------------ Line strength index definitions: ------------------------------------------------------------------ Index Bandpass Blue Sideband Red Sideband ------------------------------------------------------------------ Hdelta 4083.500-4122.250 4017.00-4057.00 4153.00-4193.00 Hgamma 4319.750-4363.500 4242.00-4282.00 4404.00-4444.00 Hbeta 4847.875-4876.625 4799.00-4839.00 4886.00-4926.00 [O II] 3716.300-3738.300 3696.30-3716.30 3738.30-3758.30 --- e_[OII] rms uncertainty on [O II] --- Notes Notes number=3 abs: galaxy with absorption lines emi: galaxy with emission lines E+A: starburst galaxy bcg+emi: brightest cluster galaxy, galaxy with emission lines emi+Hdelta: galaxy with [O II] emission and H{delta} absorption stronger than 4{AA}. --- James Marcout, Patricia Bauer CDS 1998 Aug 12 UNKNOWN UNKNOWN From ApJ electronic version J_ApJ_498_195.xml Hubble space telescope imaging of the CFRS and LDSS redshift surveys. I. Morphological properties. J/ApJ/499/112 J/ApJ/499/112 HST CFRS and LDSS redshift surveys. I. Hubble space telescope imaging of the CFRS and LDSS redshift surveys. I. Morphological properties. J Brinchmann R Abraham D Schade L Tresse R S Ellis S Lilly O Le Fevre K Glazebrook F Hammer M Colless D Crampton T Broadhurst Astrophys. J. 499 112 1998 1998ApJ...499..112B J/ApJ/455/60 : CFRS II: 0000-00 and 1000+25 fields (Le Fevre+ 1995) J/ApJ/455/75 : CFRS III: 1415+52 and 2215+00 fields (Lilly+ 1995) J/ApJ/455/88 : CFRS IV: 0300+00 field (Hammer+ 1995) J/ApJ/464/79 : CFRS XI: High-redshift field galaxies morphology (Schade+ 1996) J/ApJ/481/49 : CFRS XIV. Field galaxies up to z=1 (Hammer+ 1997) J/MNRAS/273/157 : A faint galaxy survey to B = 24. (Glazebrook+ 1995) Lilly et al., Paper II. 1998ApJ...500...75L Galaxies, photometry Redshifts Spectroscopy galaxies: fundamental parameters galaxy: structure surveys We analyze Hubble Space Telescope images of a complete sample of 341 galaxies drawn from the Canada-France Redhsift Survey (CFRS) and Low-Dispersion Survey Spectrograph (LDSS) ground-based redshift surveys. In this, the first paper in the series, each galaxy has been morphologically classified according to a scheme similar to that developed for the Medium Deep Survey. We discuss the reproducibility of these classifications and quantify possible biases that may arise from various redshift-dependent effects. We then discuss automated classifications of the sample and conclude, from several tests, that we can expect an apparent migration with redshift to later Hubble types that corresponds to a misclassification in our adopted machine classification system of ~24%+/-11 of the true "spirals" as "peculiars" at a redshift z~=0.9. After allowing for such biases, the redshift distribution for normal spirals, together with their luminosity function derived as a function of redshift, indicates approximately 1mag of luminosity evolution in B_AB_ by z~=1. The elliptical sample is too small for precise evolutionary constraints. However, we find a substantial increase in the proportion of galaxies with irregular morphology at large redshift from 9%+/-3% for 0.3<=z<=0.5 to 32%+/-12% for 0.7<=z<=0.9. These galaxies also appear to be the dominant cause of the rapid rise with redshift in the blue luminosity density identified in the redshift surveys. Although galaxies with irregular morphology may well comprise a mixture of different physical systems and might not correspond to present-day irregulars, it is clear that the apparently declining abundance and luminosities of our distant "irregulars" holds an important key to understanding recent evolution in the star formation history of normal galaxies.
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Data for objects in the survey ID Identification number --- z Redshift --- n_z Note on z number=1 g: The object is clearly extended, but was given z=0 in in the CFRS survey --- F814W F814W magnitude mag BMag Absolute B_AB_ magnitude mag n_BMag Note on BMag number=2 h: The HST photometry here is uncertain, and M_AB_ is based on the original b_J_ photometry i: The absolute magnitude is the original Autofib absolute magnitude based on b_J_ transformed to AB --- Class Redhsift confidence class number=3 Each object identification was assigned a confidence class. The notation was set to classes 0-4, 8, 9, 12-14, 91-94 as follow: 0-4: 0: when no redshift could be assigned 1: probability of 50% that the measurement was correct 2: probability of more than 75% that the measurement was correct 3: measurement at least 95% secure 4: unquestionably correct identification 8-9: 8: object for which the algorithm indicates that the emission line is [O II]{lambda}3727 9: object for which the redshift ambiguity still could not be resolved 12-14: QSO are identified with the same quality notation 1-4 as galaxies, but a 1 is placed in front, e.g., 14 is a very secure QSO. 91-94: Objects which do not belong to the main catalog, either because they have I_AB_=22.5 or I_AB_<17.5, because of instrumental problems but have a redshift determination, or whose photometry was adjusted fainter than I_AB_=22.5 after the spectroscopic observation, are kept in a supplemental catalog and are identified by a 9 in front of the confidence class, e.g., 93. The objects in this supplemental catalog may thus have biases that will not be present in the statistically complete sample. For the LDSS objects this has been transformed to the CFRS system by assigning note = 4 to confident redshifts, note = 2 to less secure redshifts, and 0 to failures. For the few LDSS objects for which there is no confidence class, we have assigned note = -1. For CFRS 03.1027, the original "39" value was modified in "9", as in table1 of Cat. <J/ApJ/455/88> --- MClass Eyeball morphological classification for the object --- A Uncorrected rotational asymmetry factor --- C Uncorrected central concentration index --- MClassAC AC morphological classification number=4 AC classification for the object using the division lines in Fig. 8. --- EW[OII] [O II] equivalent width number=5 For the CFRS objects this is from Hammer et al. (1997, Cat. <J/ApJ/481/49>); for the LDSS objects it is from the Autofib survey (Ellis et al., 1996MNRAS.280..235E) 0.1nm e_EW[OII] rms uncertainty on EW[OII] 0.1nm Origin Origin number=6 CFRS: Canada-France Redhsift Survey, Lilly et al., 1995ApJ...455...50L; Le Fevre et al. 1995, Cat. <J/ApJ/455/60> GRTH: Groth et al., 1994BAAS..185.5309G LDSS-1: Low-Dispersion Survey Spectrograph (Colless et al., 1993MNRAS.261...19C) LDSS-2: Low-Dispersion Survey Spectrograph (Glazebrook et al., 1995) Cat. <J/MNRAS/273/157>) Autofib: Autofib Survey (Ellis et al., 1996MNRAS.280..235E) --- OldID Old identification number=7 The identification given in the original LDSS paper --- James Marcout, Patricia Bauer CDS 1998 Sep 22 UNKNOWN UNKNOWN From electronic ApJ version J_ApJ_499_112.xml The millimeter- and submillimeter-wave spectrum of ethylene oxide (c-C_2_H_4_O) J/ApJ/499/517 J/ApJ/499/517 Ethylene oxide spectrum The millimeter- and submillimeter-wave spectrum of ethylene oxide (c-C_2_H_4_O) J Pan S Albert K V L N Sastry E Herbst F C De Lucia Astrophys. J. 499 517 1998 1998ApJ...499..517P J/ApJS/117/427 : Sgr B2 spectral survey (Nummelin+, 1998) J/ApJ/500/1059 : Dimethyl ether transitions frequencies (Groner+, 1998) Atomic physics Spectroscopy ISM: molecules methods: laboratory molecular data radio lines: ISM The cyclic molecule ethylene oxide (c-C_2_H_4_O) has recently been detected in the interstellar source Sgr B2N. Previous laboratory work on the rotational spectrum of this molecule extends only to a frequency of 123GHz. We report here the extension of the laboratory rotational spectrum of this species through the frequency range 262358GHz using a new fast scan spectrometer (fast scan submillimeter spectroscopic technique, FASSST). The newly measured lines have been combined with previous data at lower frequencies to form a data set consisting of 662 lines that has been assigned and fitted via a standard semirigid asymmetric top analysis. The spectral constants obtained from the fit have allowed us to predict the frequencies of many additional lines.
Assigned and fitted transition frequencies of Ethylene oxide in the ground vibrational state J' J' rotational quantum number --- K'a K'a rotational quantum number --- K'c K'c rotational quantum number --- J" J" rotational quantum number --- K"a K"a rotational quantum number --- K"c K"c rotational quantum number --- FreqM Measured frequency MHz FreqC Calculated frequency MHz O-C Measured minus calculated frequency value MHz Ref References number=1 1: Hirose, 1974ApJ...189L..45H 2: Creswell & Schwendeman, 1974, Chem. Phys. Lett. 27, 521 The lack of a reference indicates that the line is reported here for the first time --- Predicted transition frequencies of ethylene oxide in the ground vibrational state J' J' rotational quantum number --- K'a K'a rotational quantum number --- K'c K'c rotational quantum number --- J" J" rotational quantum number --- K"a K"a rotational quantum number --- K"c K"c rotational quantum number --- Freq Frequency MHz e_Freq rms uncertainty on Freq MHz mu2S Intensity ({mu}^2^S) number=1 S-value (Townes & Schawlow, 1975, Microwave Spectroscopy (New York: Dover)) multiplied by the square of the dipole moment D+2 Eu Upper state energy cm-1 James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From ApJ electronic version J_ApJ_499_517.xml Dimethyl ether: laboratory assignments and predictions through 600 GHz. J/ApJ/500/1059 J/ApJ/500/1059 Dimethyl ether transitions frequencies Dimethyl ether: laboratory assignments and predictions through 600 GHz. P Groner S Albert E Herbst F C De Lucia Astrophys. J. 500 1059 1998 1998ApJ...500.1059G J/ApJ/499/517 : Ethylene oxide spectrum (Pan+, 1998) Atomic physics Interstellar medium ISM: molecules molecular data molecular processes radio lines: ISM Dimethyl ether (CH_3_OCH_3_) is a well-known interstellar molecule with a large abundance in hot core regions. We have measured many rotational-torsional transition lines of this molecule in the 100-550GHz frequency range using two experimental techniques: a klystron-based traditional millimeter-wave spectrometer and a new fast scan spectrometer (designated "FASSST") with a voltage-tunable backward wave oscillator. The lines arising from the ground vibrational state have been combined with previous data, mainly at lower frequencies, to form a global data set consisting of over 1600 lines that have been assigned and fitted by an effective Hamiltonian method. The spectral constants obtained from the fit allow us to predict the frequencies of almost 6000 additional lines of dimethyl ether through 600GHz.
Assigned and Fitted Transition Frequencies of Dimethyl Ether in the Ground Vibrational State t Torsional substates number=1 00=AA , 01=EE , 11=AE , 12=EA --- J' J' rotational quantum number --- K'a K'a rotational quantum number --- K'c K'c rotational quantum number --- J" J" rotational quantum number --- K"a K"a rotational quantum number --- K"c K"c rotational quantum number --- Freq Frequency MHz O-C Observed minus calculated frequency MHz e_Freq rms uncertainty on Freq number=2 A 0.000 in the uncertainties column signifies that the transition has been assigned but not included in the fit. Many of these are weaker, blended lines for which the measured frequency of the stronger neighbor was used to calculate the listed O - C. A total of 1626 assigned frequencies were used in the fit. MHz Source Source number=3 L: Lovas et al. 1979, J. Phys. Chem. Ref. Data 8, 1051 D: Durig et al. 1976, J. Molec. Spectrosc. 62, 159 N: Neustock et al. 1990, Z. Naturforsch. 45a, 702 K: this work, klystron-based measurements F: this work, FASSST-based measurements --- Predicted Transition Frequencies of Dimethyl Ether in the Ground Vibrational State t Torsional substates number=1 Torsional substates: 00=AA , 01=EE , 11=AE , 12=EA --- J' J' rotational quantum number --- K'a K'a rotational quantum number --- K'c K'c rotational quantum number --- J" J" rotational quantum number --- K"a K"a rotational quantum number --- K"c K"c rotational quantum number --- Freq Frequency MHz e_Freq rms uncertainty on Freq MHz WSpin Spin weight --- S S value (Townes & Schawlow, 1975, Microwave Spectroscopy (New York: Dover))) --- Eu Upper state energies cm-1 James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From ApJ electronic version J_ApJ_500_1059.xml Evolved massive stars in the local group. I. Identification of red supergiants in NGC 6822, M31, and M33. J/ApJ/501/153 J/ApJ/501/153 VRB photometry of red supergiants Evolved massive stars in the local group. I. Identification of red supergiants in NGC 6822, M31, and M33. P Massey Astrophys. J. 501 153 1998 1998ApJ...501..153M Photometry, CCD Radial velocities Stars, supergiant galaxies: individual (NGC 6822, M 33, M 31) stars: late-type stars: Wolf-Rayet supergiants Knowledge of the red supergiant (RSG) population of nearby galaxies allows us to probe massive star evolution as a function of metallicity; however, contamination by foreground Galactic dwarfs dominates surveys for red stars in Local Group galaxies beyond the Magellanic Clouds. Model atmospheres predict that low-gravity supergiants will have B-V values that are redder by several tenths of a magnitude than foreground dwarfs at a given V-R color, a result that is largely independent of reddening. We conduct a BVR survey of several fields in the Local Group galaxies NGC 6822, M33, and M31 as well as neighboring control fields and identify RSG candidates from CCD photometry. The survey is complete to V=20.5, corresponding to M_V_=-4.5 or an M_bol_ of -6.3 for the reddest stars. Follow-up spectroscopy at the Ca II triplet of 130 stars is used to demonstrate that our photometric criterion for identifying RSGs is highly successful (96% for stars brighter than V=19.5; 82% for V=19.5-20.5). Classification spectra are also obtained for a number of stars in order to calibrate color with spectral type empirically.
Survey of red stars Star Star name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag V-R V-R colour index mag e_V-R rms uncertainty on V-R mag Class Photometric classification number=1 fgd, Fgd: foreground star rsg, RSG: red supergiant --- D(B-V) Distance from the cutoff curve mag Crd? Isolated or crowded star? number=2 "I" indicates that the star is isolated, and "C" indicates that the star is crowded, depending upon whether or not there are any stars brighter than 1.0mag fainter within 3" or any star as bright or brighter within 3"-5". --- ClassS Spectroscopyc classification number=1 fgd, Fgd: foreground star rsg, RSG: red supergiant --- SType Spectral type --- CrossID Corss-identification number=3 Cross-identifications are given for stars with previous spectroscopy by Humphreys (1980ApJ...238...65H) for NGC 6822, Humphreys (1980ApJ...241..587H) for M33, and Humphreys et al. (1988, Cat. <J/AJ/96/1884>) for M31. --- Spectroscopy of red stars Star Star name number=1 N6Con: NGC 6822 Control Field --- Vmag V magnitude mag B-V B-V colour index mag V-R V-R colour index mag Class rsg or fgd from photometry --- D(B-V) Distance from the cutoff curve mag Crd? Isolated or crowded star? number=2 "I" indicates that the star is isolated, and "C" indicates that the star is crowded, depending upon whether or not there are any stars brighter than 1.0mag fainter within 3" or any star as bright or brighter within 3"-5". --- RV Radial velocity number=4 Fields radio velocities NGC 6822-A: RV = -75km/s NGC 6822-B: RV = -55km/s NGC 6822-C: RV = -42km/s M33-A: RV = -200km/s M33-B: RV = -220km/s M33-D: RV = -155km/s M33-E: RV = -130km/s M33-F: RV = -130km/s M33-G: RV = -135km/s M31ob8: RV = -115km/s M31ob48: RV = -145km/s M31ob69: RV = -430km/s M31ob78: RV = -555km/s M31ob102: RV = -40km/s km/s u_RV Uncertainty flag on RV --- Lines Ca II triplet feature intensity number=3 "Weak," "moderate," and "strong" correspond to equivalent widths of less than 8{AA}, 8-10{AA}, and greater than 10{AA}, respectively. --- RSG? rsg or fgd from spectroscopy --- Agree? Yes, No --- SType Spectral type --- James Marcout, Patricia Bauer CDS 1998 Nov 19 UNKNOWN UNKNOWN From ApJ electronic version J_ApJ_501_153.xml Color-luminosity relations for the resolved hot stellar populations in the centers of M31 and M32. J/ApJ/504/113 J/ApJ/504/113 F175W and F275W photometry of M31 and M32 Color-luminosity relations for the resolved hot stellar populations in the centers of M31 and M32. T M Brown H C Ferguson S A Stanford J Deharveng Astrophys. J. 504 113 1998 1998ApJ...504..113B J/ApJ/324/172 : M31 UBVR photometry (Hodge+, 1988) Galaxies, photometry Photometry, ultraviolet galaxies: evolution galaxies: individual (M31, M32) galaxies: stellar content Hertzsprung-Russel diagram ultraviolet: galaxies We present Faint Object Camera (FOC) ultraviolet images of the central 14"x14" of Messier 31 and Messier 32. The hot stellar populations detected in the composite UV spectra of these nearby galaxies are partially resolved into individual stars, and their individual colors and apparent magnitudes are measured. We detect 433 stars in M31 and 138 stars in M32, down to detection limits m_F275W_=25.5mag and m_F175W_=24.5mag.
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M31 source catalog M32 source catalog RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign (J2000) --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec mF175W F175W magnitude mag u_mF175W Uncertainty flag on mF175W --- e_mF175W rms uncertainty on mF175W mag mF275W F275W magnitude mag u_mF275W Uncertainty flag on mF275W --- e_mF275W rms uncertainty on mF275W mag Note Note number=1 a: Brightest star b: Second brightest star Photometric problems are discussed in Sec. 2 and Sec. 3.2. --- James Marcout, Patricia Bauer CDS 1998 Oct 05 UNKNOWN UNKNOWN From ApJ electronic version J_ApJ_504_113.xml Quantitative morphology of galaxies in the Hubble Deep Field. J/ApJ/507/585 J/ApJ/507/585 Hubble Deep Field galaxy morphology Quantitative morphology of galaxies in the Hubble Deep Field. F R Marleau L Simard Astrophys. J. 507 585 1998 1998ApJ...507..585M J/AJ/112/359 : Galaxies in the Hubble Deep Field (van den Bergh+ 1996) J/AJ/112/1335 : Hubble Deep Field observations (Williams+ 1996) J/A+AS/129/583 : Hubble Deep Field surface photometry (Fasano+ 1998) Galaxies, photometry Morphology galaxies: evolution galaxies: formation galaxies: fundamental parameters We measure quantitative structural parameters of galaxies in the Hubble deep field (HDF) on the drizzled F814W images. Our structural parameters are based on a two-component surface brightness made up of a Sirsic profile and an exponential profile. We compare our results to the visual classification of van den Bergh et al. (1996, Cat. <J/AJ/112/359>) and the C-A classification of Abraham et al. (1996MNRAS.279L..47A). Our morphological analysis of the galaxies in the HDF indicates that the spheroidal galaxies, defined here as galaxies with a dominant bulge profile, make up for only a small fraction, namely, 8%, of the galaxy population down to m_F814W_(AB)=26.0. We show that the larger fraction of early-type systems in the van den Bergh sample is primarily due to the difference in classification of 40% of small round galaxies with half-light radii less than 031. Although these objects are visually classified as elliptical galaxies, we find that they are disk dominated with bulge fractions less than 0.5. Given the existing large data set of HDF galaxies with measured spectroscopic redshifts, we are able to determine that the majority of distant galaxies (z>2) from this sample are disk dominated. Our analysis reveals a subset of HDF galaxies that have profiles flatter than a pure exponential profile.
HST
Best morphological parameter values and their confidence limits for galaxies with m_F814W_<=26.0 in the HDF [MS98b] Identification (hdchp_x_y) --- mF814W F814W magnitude mag E_mF814W Error on mF814W (Upper limit) mag e_mF814W Error on mF814W (Lower limit) mag B/T Bulge fraction (0 = pure disk system) --- E_B/T Error on B/T (Upper limit) --- e_B/T Error on B/T (Lower limit) --- re Bulge effective radius arcsec E_re Error on re (Upper limit) arcsec e_re Error on re (Lower limit) arcsec e Bulge ellipticity (1-b/a) --- E_e Error on e (Upper limit) --- e_e Error on e (Lower limit) --- Phib Bulge position angle of the major axis (clockwise, 0 = y-axis) deg E_Phib Error on Phib (Upper limit) deg e_Phib Error on Phib (Lower limit) deg rd Exponential disk scale length arcsec E_rd Error on rd (Upper limit) arcsec e_rd Error on rd (Lower limit) arcsec i Disk inclination (0 = face-on) deg E_i Error on i (Upper limit) deg e_i Error on i (Lower limit) deg Phid Disk position angle deg E_Phid Error on Phid (Upper limit) deg e_Phid Error on Phid (Lower limit) deg rh Half-light radius arcsec xi2R Reduced chi-square {chi}^2^_R_ --- vdB van den Bergh (1996, Cat. <J/AJ/112/359>) classification --- Sersic parameters and color gradients for 82 galaxies in the HDF [MS98b] Identification (hdchp_x_y) --- n Sersic number --- E_n Error on n (Upper limit) --- e_n Error on n (Lower limit) --- chi2R Sersic {chi}^2^_R_ value --- (V-I)G (V-I) gradient --- vdB van den Berg (1996, Cat. <J/AJ/112/359>) classification --- James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From electronic version J_ApJ_507_585.xml The Hubble Space Telescope Key Project on the extragalactic distance scale. XII. The discovery of cepheids and a new distance to NGC 2541. J/ApJ/507/655 J/ApJ/507/655 VI photometry of new Cepheids in NGC 2541 The Hubble Space Telescope Key Project on the extragalactic distance scale. XII. The discovery of cepheids and a new distance to NGC 2541. L Ferrarese F Bresolin R C Kennicutt Jr. A Saha P B Stetson W L Freedman J R Mould B F Madore S Sakai H C Ford B K Gibson J A Graham M Han J G Hoessel J Huchra S M Hughes G D Illingworth R Phelps C F Prosser N A Silbermann Astrophys. J. 507 655 1998 1998ApJ...507..655F Photometry Stars, variable Cepheids galaxies: distances and redshifts galaxies: individual (NGC 2541) We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.
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Astrometry for the NGC 2541 Cepheids Astrometry for other NGC 2541 variable candidates [FBK98] Identification (CNN or VNN) number=1 CNN for Cepheids stars, VNN for other variable stars --- Xpos X position number=2 The X- and Y-coordinates are relative to the 1995 October 30 epoch. For each 800 x 800 pixels chip, pixel [1, 1] is located at the edge of the pyramid. pix Ypos Y position number=2 The X- and Y-coordinates are relative to the 1995 October 30 epoch. For each 800 x 800 pixels chip, pixel [1, 1] is located at the edge of the pyramid. pix RAh Right ascension (J2000) number=3 RA and DE are calculated using the IRAF task STSDAS.HST CALIB.WFPC.METRIC, version 1.3.5 (1996 July). h RAm Right ascension (J2000) number=3 RA and DE are calculated using the IRAF task STSDAS.HST CALIB.WFPC.METRIC, version 1.3.5 (1996 July). min RAs Right ascension (J2000) number=3 RA and DE are calculated using the IRAF task STSDAS.HST CALIB.WFPC.METRIC, version 1.3.5 (1996 July). s DE- Declination sign (J2000) --- DEd Declination (J2000) number=3 RA and DE are calculated using the IRAF task STSDAS.HST CALIB.WFPC.METRIC, version 1.3.5 (1996 July). deg DEm Declination (J2000) number=3 RA and DE are calculated using the IRAF task STSDAS.HST CALIB.WFPC.METRIC, version 1.3.5 (1996 July). arcmin DEs Declination (J2000) number=3 RA and DE are calculated using the IRAF task STSDAS.HST CALIB.WFPC.METRIC, version 1.3.5 (1996 July). arcsec Chip Chip (PC, WF 2, WF 3, WF 4) --- V (F555W) photometry for NGC 2541 Cepheids I (F814W) photometry for NGC 2541 Cepheids V photometry for other NGC 2541 variable candidates I photometry for other NGC 2541 variable candidates [FBK98] Identification (CNN or VNN) --- HJD Heliocentric Julian date d mag V or I magnitude mag e_mag rms uncertainty on mag mag DOPHOT mean photometry of the NGC 2541 Cepheids Allframe mean photometry of the NGC 2541 Cepheids DOPHOT mean photometry of other NGC 2541 variables Allframe mean photometry of other NGC 2541 variables [FBK98] Identification (CNN or VNN) --- l_Per Limit flag on Per --- Per Period d l_Per2 Limit flag on Per2 --- Per2 Upper limit for period interval d F555Wph Phase-weighted mean F555W magnitude mag F555Wav Intensity-averaged mean F555W magnitude mag F814Wph Phase-weighted mean F814W magnitude mag F814WphCor Correction adopted for F814Wph number=1 Value of the magnitude correction applied to the F814W magnitudes, defined as in section 4.4 of the paper. mag F814Wav Intensity-average mean F814W magnitude mag F814WavCor Correction adopted for F814Wav number=1 Value of the magnitude correction applied to the F814W magnitudes, defined as in section 4.4 of the paper. mag Vmagph Phase-weighted mean V magnitude mag Vmagav Intensity-averaged mean V magnitude mag Imagph Phase-weighted mean I magnitude mag Imagav Intensity-averaged mean I magnitude mag chi2/sigma Reduced {xi}^2^_r_ value for DoPHOT or {sigma} for ALLFRAME --- I (F814W) photometry for NGC 2541 Cepheids DOPHOT mean photometry of the NGC 2541 Cepheids Allframe mean photometry of the NGC 2541 Cepheids Photometry for the WF4 secondary standards Xpos X position number=1 The X and Y coordinate are relative to the 1995 October 30 epoch. For each 800x800 pixels chip, pixel [1,1] is located at the edge of the WFPC2 pyramid pix Ypos Y position number=1 The X and Y coordinate are relative to the 1995 October 30 epoch. For each 800x800 pixels chip, pixel [1,1] is located at the edge of the WFPC2 pyramid pix RAh Right ascension (J2000) number=2 RA and DE are calculated using the IRAF task STSDAS.HST_CALIB.WFPC.METRIC, version 1.3.5 (July 1996) h RAm Right ascension (J2000) number=2 RA and DE are calculated using the IRAF task STSDAS.HST_CALIB.WFPC.METRIC, version 1.3.5 (July 1996) min RAs Right ascension (J2000) number=2 RA and DE are calculated using the IRAF task STSDAS.HST_CALIB.WFPC.METRIC, version 1.3.5 (July 1996) s DE- Declination sign (J2000) number=2 RA and DE are calculated using the IRAF task STSDAS.HST_CALIB.WFPC.METRIC, version 1.3.5 (July 1996) --- DEd Declination (J2000) number=2 RA and DE are calculated using the IRAF task STSDAS.HST_CALIB.WFPC.METRIC, version 1.3.5 (July 1996) deg DEm Declination (J2000) number=2 RA and DE are calculated using the IRAF task STSDAS.HST_CALIB.WFPC.METRIC, version 1.3.5 (July 1996) arcmin DEs Declination (J2000) number=2 RA and DE are calculated using the IRAF task STSDAS.HST_CALIB.WFPC.METRIC, version 1.3.5 (July 1996) arcsec F555W F555W magnitude(3) mag e_F555W rms uncertainty on F555W mag F814W F814W magnitude number=3 F555W and F814W instrumental magnitudes are intensity averaged over 13 and 5 epochs respectively. mag e_F814W rms uncertainty on F814W mag Vmag V magnitude number=4 V and I magnitudes are calculated from the instrumental F555W and F814W magnitudes as described in section 3 of the paper. mag Imag I magnitude number=4 V and I magnitudes are calculated from the instrumental F555W and F814W magnitudes as described in section 3 of the paper. mag Individual notes on Cepheids Individual notes on other variable stars [FBK98] Identification (CNN or VNN) --- Note Text of the note number=1 The term "isolated" is use d for stars for which no companions are identified within a 3 pixel radius. --- Patricia Bauer CDS 1999 Mar 09 From ApJ electronic version J_ApJ_507_655.xml A catalog of stellar velocity dispersions. II. 1994 update J/ApJS/100/105 J/ApJS/100/105 Stellar velocity dispersions. II. A catalog of stellar velocity dispersions. II. 1994 update D B McElroy Astrophys. J. Suppl. Ser. 100 105 1995 1995ApJS..100..105M VII/72 : Catalog of stellar velocity dispersions. I. (Whitmore+ 1985) J/A+AS/113/151 : Elliptical galaxies velocity dispersions (Di Nella+, 1995) J/ApJ/368/54 : E and S0 galaxies velocities and photometry (Dressler+ 1991) Galaxy catalogs Velocity dispersion catalogs galaxies: kinematics and dynamics A catalog of central velocity dispersion measurements is presented, current through 1993 September. The catalog includes 2474 measurements of 1563 (*) galaxies. A standard set of 86 galaxies is defined, consisting of galaxies with at least three reliable concordant measurements. It is suggested that future studies observe some of these standard galaxies so that different studies can be normalised to a consistent system. All measurements are reduced to a normalized system using these standards. (*) Actually 1562 galaxies.
Catalog velocity dispersions Name Galaxy name --- n_Name Note on NGC 4486 number=1 NGC 4486 has two velocity dispersions --- MType Morphological type --- n_MType Note on MType number=2 The morphological types marked with an asterisk are from Nilson (1973, Cat. <VII/26>), else from the RC3 (Cat. <VII/155>) --- sigma Velocity dispersion km/s James Marcout, Patricia Bauer CDS 1998 Mar 23 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_100_105.xml An Out-of-Plane CO (J = 2-1) Survey of the Milky Way. I. The Data J/ApJS/100/125 J/ApJS/100/125 CO An Out-of-Plane CO (J = 2-1) Survey of the Milky Way. I. The Data S Sakamoto T Hasegawa M Hayashi T Handa T Oka Astrophys. J. Suppl. Ser. 100 125 1995 1995ApJS..100..125S Carbon monoxide Radio sources Galaxy: structure ISM: molecules surveys This extensive survey of the first quadrant of the Galaxy (GLON from 20 to 60 degrees, GLAT from -1 to +1 degrees) was taken with the 60-cm submillimiter-wave telescope of the University of Tokyo-Nobeyama Radio Observatory. The HPBW (half-power beam width) is 9+/-1 arcmin at 230GHz, and the intensity scale of the data is stable within typical fluctuations of 5%. It was carried out between December 1992 and May 1993. The survey gives the main-beam brightness temperatures (sensitivity of 0.4K) on a grid spaced every 15' (0.25 deg) in GLON and GLAT, and velocities spaced every 0.65km/s between -13 and 153 km/s (velocity resolution of 0.3km/s)
CO(J=2-1) longitude-velocity map of b=+0.000 CO(J=2-1) longitude-velocity map of b=+0.250 CO(J=2-1) longitude-velocity map of b=+0.500 CO(J=2-1) longitude-velocity map of b=+0.750 CO(J=2-1) longitude-velocity map of b=+1.000 CO(J=2-1) longitude-velocity map of b=-0.250 CO(J=2-1) longitude-velocity map of b=-0.500 CO(J=2-1) longitude-velocity map of b=-0.750 CO(J=2-1) longitude-velocity map of b=-1.000 GLON Galactic longitude deg Tmb Array of Intensity of CO(J=2-1) emission number=1 main-beam brightness temperatures corrected for the atmospheric attenuation and the main beam efficiency of the antenna (0.93) for 256 velocities defined by: (-12.950 + 0.650 * (I-1)), I=1,256 (km/s). K Toshihiro Horaguchi Japan 1996 Feb 23 Seiichi Sakamoto <seiichi@nro.nao.ac.jp> http://www.nro.nao.ac.jp/~seiichi J_ApJS_100_125.xml The Second Caltech-Jodrell Bank VLBI Survey. II. Observations of 102 of 193 Sources J/ApJS/100/1 J/ApJS/100/1 Second Caltech-Jodrell Bank VLBI Survey. II. The Second Caltech-Jodrell Bank VLBI Survey. II. Observations of 102 of 193 Sources D R Henstock I W A Browne P N Wilkinson G B Taylor R C Vermeulen T J Pearson A C S Readhead Astrophys. J. Suppl. Ser. 100 1 1995 1995ApJS..100....1H J/ApJS/98/1 : First Caltech-Jodrell Bank VLBI Survey. I (Polatidis+ 1995) J/ApJS/98/33 : First Caltech-Jodrell Bank VLBI Survey. II (Thakkar+ 1995) J/ApJS/99/297 : First Caltech-Jodrell Bank VLBI Survey. III (Xu+ 1995) J/ApJS/95/345 : Second Caltech-Jodrell Bank VLBI Survey. I. (Taylor+ 1994) QSOs Radio sources VLBI galaxies: structure quasars: general radio continuum: galaxies surveys techniques: interferometric This is the second of two papers presenting the Second Caltech- Jodrell Bank VLBI survey (CJ2). The CJ2 sample consists of 193 flat- and gigahertz-peaked-spectrum sources selected at 4850 MHz. In this paper we present images of the remaining 102 sources with ~1 mas resolution, obtained using VLBI snapshot observations at 4992 MHz with a global array. We also present integrated radio spectra for the entire CJ2 sample.
Map parameters Source B1950 source name according to IAU convention --- Date Date of VLBI observation --- Dur Duration on source of VLBI observation min a FWHM of major axis of the restoring beam mas b FWHM of minor axis of the restoring beam mas PA Position angle of major axis, north through east deg S4.85GHzn Peak flux density, naturally weighted map Data are in mJy/beam mJy e_S4.85GHzn Off source rms, naturally weighted map mJy S4.85GHznC First contour, percent of peak flux density % S4.85GHzt Peak flux density, tapered map mJy e_S4.85GHzt Off source rms, tapered map mJy S4.85GHztC First contour, % of peak flux density % Gaussian models CJ2 B1950 source name according to IAU convention --- S Flux density of component Jy Rad Radius of component Radius of component, measured from position of first component. mas Theta Angle to component Angle to component, measured north through east from the position of the first component. deg a FWHM of major axis of component mas b/a Axial ratio of major to minor axis, b/a --- Phi Position angle of major axis, north through east deg Amp Amplitude agreement factor --- Phase Closure phase agreement factor --- Total Total agreement factor --- Patricia Bauer CDS 1996 Oct 14 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 10-May-95 J_ApJS_100_1.xml Cosmic background anisotropies in cold dark matter cosmology J/ApJS/100/281 J/ApJS/100/281 Cosmic background anisotropies Cosmic background anisotropies in cold dark matter cosmology N Sugiyama Astrophys. J. Suppl. Ser. 100 281 1995 1995ApJS..100..281S Models, evolutionary cosmic microwave background cosmology: theory dark matter The data are normalized to a sigma(10 deg) of 30 muK. Cosmic microwave background (CMB) anisotropies and density fluctuations are calculated for flat cold dark matter (CDM) models with a wide range of parameters, viz., {OMEGA}_0,h_, and {OMEGA}_B_, for standard recombination and for various epochs of reionization. Tables of the power spectrum of CMB anisotropies in the form of C_l_ values as a function of l are presented. Although the Harrison-Zeldovich initial spectrum is assumed in these tables, we present simple approximations for obtaining the C_l_ values corresponding to a tilted spectrum from those with a Harrison-Zeldovich spectrum. Values of {sigma}_8_ are derived for the matter density spectrum, with {sigma}(10deg), fixed Q_(rms-PS) and COBE Differential Microwave Radiometer (DMR) 2yr normalizations. Simple modifications of the fitting formula for the density transfer function are given which are applicable for models with high baryon density. By using both numerical results and these fitting formulae, we calculate the relation between {sigma}_8_ and Q_(rms-PS) and find good agreement. In addition, the velocity fields are calculated.
10^10^xl(l+1)C_l_/2{pi} for h=0.3 and {OMEGA}_0_=1 l Model parameter, l --- OBs_01 Standard recombination, {OMEGA}_B_=0.01 --- OBs_03 Standard recombination, {OMEGA}_B_=0.03 --- OBs_06 Standard recombination, {OMEGA}_B_=0.06 --- OBs_10 Standard recombination, {OMEGA}_B_=0.10 --- OBs_14 Standard recombination, {OMEGA}_B_=0.14 --- OBr_01 Reionization (tau=1), {OMEGA}_B_=0.01 --- OBr_03 Reionization (tau=1), {OMEGA}_B_=0.03 --- OBr_06 Reionization (tau=1), {OMEGA}_B_=0.06 --- OBr_10 Reionization (tau=1), {OMEGA}_B_=0.10 --- OBr_14 Reionization (tau=1), {OMEGA}_B_=0.14 --- 10^10^xl(l+1)C_l_/2{pi} for h=0.5 and {OMEGA}_0_=1 l Model parameter, l --- OBs_01 Standard recombination, {OMEGA}_B_=0.01 --- OBs_03 Standard recombination, {OMEGA}_B_=0.03 --- OBs_05 Standard recombination, {OMEGA}_B_=0.05 --- OBs_06 Standard recombination, {OMEGA}_B_=0.06 --- OBs_10 Standard recombination, {OMEGA}_B_=0.10 --- OBr_01 Reionization (tau=1), {OMEGA}_B_=0.01 --- OBr_03 Reionization (tau=1), {OMEGA}_B_=0.03 --- OBr_05 Reionization (tau=1), {OMEGA}_B_=0.05 --- OBr_06 Reionization (tau=1), {OMEGA}_B_=0.06 --- OBr_10 Reionization (tau=1), {OMEGA}_B_=0.10 --- 10^10^xl(l+1)C_l_/2{pi} for h=0.8 and {OMEGA}_0_=1 l Model parameter, l --- OBs_01 Standard recombination, {OMEGA}_B_=0.01 --- OBs_02 Standard recombination, {OMEGA}_B_=0.02 --- OBs_03 Standard recombination, {OMEGA}_B_=0.03 --- OBs_06 Standard recombination, {OMEGA}_B_=0.06 --- OBs_10 Standard recombination, {OMEGA}_B_=0.10 --- OBr_01 Reionization (tau=1), {OMEGA}_B_=0.01 --- OBr_02 Reionization (tau=1), {OMEGA}_B_=0.02 --- OBr_03 Reionization (tau=1), {OMEGA}_B_=0.03 --- OBr_06 Reionization (tau=1), {OMEGA}_B_=0.06 --- OBr_10 Reionization (tau=1), {OMEGA}_B_=0.10 --- 10^10^xl(l+1)C_l_/2{pi} for h=0.5, {OMEGA}_0_=0.1 and {lambda}=0.9 10^10^xl(l+1)C_l_/2{pi} for h=0.5, {OMEGA}_0_=0.2 and {lambda}=0.8 10^10^xl(l+1)C_l_/2{pi} for h=0.5, {OMEGA}_0_=0.3 and {lambda}=0.7 10^10^xl(l+1)C_l_/2{pi} for h=0.5, {OMEGA}_0_=0.4 and {lambda}=0.6 l Model parameter, l --- OBs_01 Standard recombination, {OMEGA}_B_=0.01 --- OBs_03 Standard recombination, {OMEGA}_B_=0.03 --- OBs_05 Standard recombination, {OMEGA}_B_=0.05 --- OBs_06 Standard recombination, {OMEGA}_B_=0.06 --- OBr_01 Reionization (tau=1), {OMEGA}_B_=0.01 --- OBr_03 Reionization (tau=1), {OMEGA}_B_=0.03 --- OBr_05 Reionization (tau=1), {OMEGA}_B_=0.05 --- OBr_06 Reionization (tau=1), {OMEGA}_B_=0.06 --- 10^10^xl(l+1)C_l_/2{pi} for h=0.8, {OMEGA}_0_=0.1 and {lambda}=0.9 10^10^xl(l+1)C_l_/2{pi} for h=0.8, {OMEGA}_0_=0.2 and {lambda}=0.8 10^10^xl(l+1)C_l_/2{pi} for h=0.8, {OMEGA}_0_=0.3 and {lambda}=0.7 10^10^xl(l+1)C_l_/2{pi} for h=0.8, {OMEGA}_0_=0.4 and {lambda}=0.6 l Model parameter, l --- OBs_01 Standard recombination, {OMEGA}_B_=0.01 --- OBs_02 Standard recombination, {OMEGA}_B_=0.02 --- OBs_03 Standard recombination, {OMEGA}_B_=0.03 --- OBs_06 Standard recombination, {OMEGA}_B_=0.06 --- OBr_01 Reionization (tau=1), {OMEGA}_B_=0.01 --- OBr_02 Reionization (tau=1), {OMEGA}_B_=0.02 --- OBr_03 Reionization (tau=1), {OMEGA}_B_=0.03 --- OBr_06 Reionization (tau=1), {OMEGA}_B_=0.06 --- 10^10^xl(l+1)C_l_/2{pi} for {OMEGA}_0_.h approx. 0.25 and Omega_B_.h^2^=0.125 l Model parameter, l --- Os_02 Std recombination, {OMEGA}_0_=0.2, h=1.0 --- Os_03 Std recombination, {OMEGA}_0_=0.3, h=0.833 --- Os_04 Std recombination, {OMEGA}_0_=0.4, h=0.625 --- Os_05 Std recombination, {OMEGA}_0_=0.5, h=0.5 --- Or_02 Reion. (tau=1), {OMEGA}_0_=0.2, h=1.0 --- Or_03 Reion. (tau=1), {OMEGA}_0_=0.3, h=0.833 --- Or_04 Reion. (tau=1), {OMEGA}_0_=0.4, h=0.625 --- Or_05 Reion. (tau=1), {OMEGA}_0_=0.5, h=0.5 --- 10^10^xl(l+1)C_l_/2{pi} for h=0.5, {OMEGA}_0_=1 and {OMEGA}_B_=0.05 l Model parameter, l --- tau_05 Tau=0.5 --- tau_08 Tau=0.8 --- tau_15 Tau=1.5 --- tau_20 Tau=2.0 --- CDS 1996 Feb 02 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 25-Sep-95 J_ApJS_100_281.xml Pre-main-sequence evolution in the Taurus-Auriga molecular cloud J/ApJS/101/117 J/ApJS/101/117 UBVRIJHKLMNQ photometry in Taurus-Auriga Pre-main-sequence evolution in the Taurus-Auriga molecular cloud S J Kenyon L Hartmann Astrophys. J. Suppl. Ser. 101 117 1995 1995ApJS..101..117K Photometry Stars, pre-main sequence infrared: stars ISM: clouds stars: evolution stars: luminosity function, mass function stars: pre-main sequence Tables A1-A2 list average V and K magnitudes and broadband optical and near-infrared colors for T Tauri stars in the Taurus-Auriga cloud. The quoted errors are 1 sigma dispersions from the average values for objects with 2 or more measurements at V, K, or the appropriate color. For convenience, the authors quote dispersions of 0.00 for objects with only a single measurement. The last columns of Tables A1-A2 list the number of V, K, and N measurements used to compute the average values. The number of data points used to determine average colors is usually close to the number of V or K measurements. Table A3 lists IRAS colors for the Taurus-Auriga sample. For each IRAS source, the authors compiled fluxes from version 2 of the Point Source Catalog, IRAS ADDSCANs, and the IRAS Serendipitous Survey Catalog and averaged fluxes for sources appearing in 2 or 3 catalogs (see section 2 of the printed paper). The authors adopted flux zero points of Fnu(12um)=28.3Jy, Fnu(25um)=6.73Jy, Fnu(60um)=1.19Jy, and Fnu(100um)=0.43Jy to compute IRAS magnitudes and then derived colors using average K magnitudes from Table A2. In some cases, two or more pre-main-sequence stars fall in a typical IRAS beam. The authors summed the K flux of the individual objects to compute a combined K magnitude and color for these IRAS sources. These IRAS colors assume _no_ color correction for the IRAS flux. Table A4 lists various quantities derived from published spectra and the photometry in Tables A1-A3. Infrared colors and the ratio of far-IR to bolometric luminosity set the spectral energy distribution class, SED. The optical spectral type usually was taken from the literature (Herbig & Bell (1988LicOB1111....1H)) or the authors own work. The effective temperature, Teff, is based on compilations by Schmidt-Kaler (1982) and Straizys (1992). The authors estimated optical extinctions, A_V, from comparisons between the observed optical or infrared colors and colors for normal main sequence stars in Table A5. The authors adopted Bessell & Brett's (1988PASP..100.1134B) extinction curve to derive A_V from the optical color excess and to derive the extinction at 1.25um, A_J. The stellar luminosity, L_J, follows from the observed J magnitude, the extinction, and an appropriate bolometric correction from Table A5 for a distance of d=140pc. The 7-135um luminosity, L_FIR, and the bolometric luminosity, L_b, are both integrations over the reddening-corrected flux distribution. The 7-135um luminosity is quoted as an upper limit for sources not detected by IRAS. Lower limits on L_b are quoted for sources with incomplete photometry. Table A5 lists adopted broadband colors for main sequence stars. For the optical colors, this list is based on data compiled by Johnson (1966, ARA&A, 4, 193; U-B, B-V, V-R_J, and V-J_C), Schmidt-Kaler ((1982) ; U-B and B-V), and Bessell ((1990A&AS...83..357B) and 1990, PASP, 102, 1181; U-B, B-V, V-R_C, and V-I_C). Bessell & Brett (1988PASP..100.1134B) contains the most comprehensive list of main sequence IR colors. The authors supplemented their Table II with colors from Johnson (1966, ARA&A, 4, 193) for early-type main sequence stars. Johnson (1966, ARA&A, 4, 193) contains the best list of K-N colors for main sequence stars. To complement these data, the authors compiled V-[12] colors using stars selected from the Third Catalog of Nearby Stars (Gliese & Jahreiss 1979A&AS...38..423G). The authors extracted 12um fluxes from version 2 of the IRAS Point Source Catalog, color-corrected the fluxes assuming a color temperature equal to the stellar effective temperature, and computed a V-[12] color assuming a 12um zero point of 28.3Jy. The tabulated color is the median color. The tabulated visual bolometric corrections, BC_V=M_bol-M_V, were used to derive absolute J luminosities, L_J. The authors adopted BC_V from Schmidt-Kaler (1982; also Straizys 1992) for stars with spectral types earlier than K6; the authors integrated the energy distribution over wavelength to derive BC_V for for later spectral types. This paper analyzes optical and infrared photometry of pre-main- sequence stars in the Taurus-Auriga molecular cloud. More than half of the stars in our sample have excess near-infrared emission. The near-infrared excesses correlate very well with other measures of activity, such as Halpha emission, ultraviolet excess emission, millimeter continuum emission, and the presence of reflection nebulae and molecular outflows. The infrared colors and the ratio of far-infrared to bolometric luminosity display a smooth progression from the most deeply embedded protostars to optically visible T Tauri stars. Infalling envelope models account for the colors of protostars; simple disk models similarly reproduce the colors of many T Tauri stars. Both the stellar birth line and a 10^5yr isochrone provide a reasonable upper envelope to the luminosity distribution of optically visible stars in the H-R diagram. Only a few stars in the cloud have apparent ages exceeding 2-3x10^6yr, as derived from detailed stellar evolution calculations. The distribution of stars in the H-R diagram indicates that the cloud has formed stars at a roughly constant rate for the past 1-2x10^6yr. Analyses of the J- and K-luminosity functions support this conclusion. Within the uncertainties, the observed mass distribution for optically visible stars agrees with a Miller-Scalo initial mass function. Source statistics imply a lifetime of 1-2x10^5yr for the typical protostar in Taurus-Auriga. There is no evidence, however, that these sources lie on the stellar birth line. Indeed, the protostellar luminosity function is essentially identical to the luminosity function derived for optically visible T Tauri stars in the cloud. These results provide some support for the evolutionary sequence -- embedded protostar -> T Tauri star with a circumstellar disk -> T Tauri star without a circumstellar disk -- currently envisioned in standard models of low-mass star formation. Source statistics and infrared color-color diagrams demonstrate that pre-main-sequence stars develop bluer colors and display less evidence for circumstellar material with time. The data show little evidence, however, for the luminosity evolution expected along the proposed evolutionary sequence. Time-dependent accretion during the infall phase may account for the low luminosity of Taurus-Auriga protostars; this hypothesis requires more tests.
Mean optical photometry Name Star name --- Vmag Average V magnitude mag e_Vmag V error The quoted errors are 1 sigma dispersions from the average values for objects with 2 or more measurements. For convenience the dispersions are 0.00 for objects with only a single measurement (N_V=1). mag U-B Average U-B color mag e_U-B U-B error mag B-V Average B-V color mag e_B-V B-V error mag V-R Average V-R color mag e_V-R V-R error mag R-I Average R-I color mag e_R-I R-I error mag o_Vmag Number of V measurements for average The number of data points used to determine average colors is usually close to the number of V measurements --- Mean near-IR photometry Name Star name --- Kmag Average K magnitude mag e_Kmag K error The quoted errors are 1 sigma dispersions from the average values for objects with 2 or more measurements. For convenience the dispersions are 0.00 for objects with only a single measurement (N_V=1). mag J-K Average J-K color mag e_J-K J-K error mag H-K Average H-K color mag e_H-K H-K error mag K-L Average K-L color mag e_K-L K-L error mag K-M Average K-M color mag e_K-M K-M error mag K-N Average K-N color mag e_K-N K-N error mag K-Q Average K-Q color mag e_K-Q K-Q error mag o_Kmag Number of K measurements for average The number of data points used to determine average colors is usually close to the number of K measurements --- o_Nmag Number of N measurements for average --- Far-IR colors Name Star names --- K-12 K-12 um color mag K-25 K-25 um color mag K-60 K-60 um color mag K-100 K-100 um color mag Luminosities and extinctions Name Star name --- SED Spectral energy distribution class --- Sp Spectral type --- Teff Effective temperature K AV Optical extinction mag AJ Extinction at 1.25 um mag LJ Stellar luminosity The stellar luminosity, LJ, follows the J magnitude, the extinction and an appropriate bolometric correction from Table A5 for a distance of d=140pc. solLum l_LFIR L_FIR limiting character Luminosity is an upper limit, "<", for sources not detected by IRAS. --- LFIR 7-135 um luminosity solLum l_Lb L_b limiting character Luminosity is a lower limit, ">", for sources with an incomplete photometry. --- Lb Bolometric luminosity solLum l_LJ/Lb L_J/L_b limiting character --- LJ/Lb L_J/L_b ratio --- l_LFIR/Lb L_FIR/L_b limiting character --- LFIR/Lb L_FIR/L_b ratio --- Colors for main-sequence stars Sp Spectral type --- Teff Effective temperature K BC Bolometric correction mag U-V U-V color mag B-V B-V color mag V-Rc V-R(Cousins) color mag V-Rj V-R(Johnson) color mag V-Ic V-I(Cousins) color mag V-Ij V-I(Johnson) color mag V-J V-J color mag V-H V-H color mag V-K V-K color mag V-L V-L color mag V-M V-M color mag V-N V-N color mag V-12 V-12 um color mag table.tex AASTeX version of tables A1-A5 CDS 1996 Feb 02 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 06-Nov-95 J_ApJS_101_117.xml H II region populations in Seyfert galaxies. I. Database J/ApJS/101/287 J/ApJS/101/287 H II Regions in Seyfert galaxies. I. H II region populations in Seyfert galaxies. I. Database Z I Tsvetanov A R Petrosian Astrophys. J. Suppl. Ser. 101 287 1995 1995ApJS..101..287T Galaxies, Seyfert H II regions galaxies: Seyfert HII regions surveys Data on positions, effective diameters, and absolute fluxes of H II regions on 21 Seyfert spiral galaxies are presented together with the Halpha + [N II] images and identification charts. The objects are selected from a larger emission-line survey of a distance-limited sample of southern Seyfert galaxies. Statistical analysis of the data as well as discussion and comparison of the H II region populations in Seyfert and normal galaxies will be presented in forthcoming papers.
Basic characteristics of the sample galaxies (table 2) Galaxy Galaxy name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec AGN AGN type --- Morph Morphology --- cz Redshift km/s mB m_B magnitude mag HII H II region --- H II regions catalog Name Galaxies name --- Num Reference number --- X X offset of H II region The X,Y positions of the H II regions. The coordinate systems are centered on the nuclei of the galaxies, which are determined as the brightest point in Halpha. The X-axis is along the east-west direction, with negative values to the east, and the Y-axis is along the north-south direction, with negative values to the south. arcsec Y Y offset of H II region arcsec Deff Effective diameter of the H II region arcsec Flux Halpha+[N II] flux of the H II region mW/m2 CDS 1996 Sep 06 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 23-Apr-96 J_ApJS_101_287.xml A revised and extended catalog of Magellanic system clusters, associations, and emission nebulae. I. Small Magellanic Cloud and Bridge. J/ApJS/101/41 J/ApJS/101/41 SMC and Bridge extended catalog A revised and extended catalog of Magellanic system clusters, associations, and emission nebulae. I. Small Magellanic Cloud and Bridge. E L D Bica H R Schmitt Astrophys. J. Suppl. Ser. 101 41 1995 1995ApJS..101...41B Associations, stellar Magellanic Clouds Nebulae Surveys Magellanic Clouds open clusters and associations: general surveys A survey of extended objects in the Magellanic System was carried out on the ESO/SERC R and J Sky Survey Atlases. The present work is dedicated to the Small Magellanic Cloud and to the inter-Magellanic Cloud region ("Bridge") totaling 1188 objects, of which 554 are classified as star clusters, 343 are emissionless associations, and 291 are related to emission nebulae. The survey includes cross-identifications among catalogs, and we present 284 new objects. We provide accurate positions, classification, homogeneous sizes, and position angles, as well as information on cluster pairs and hierarchical relation for superimposed objects. Two clumps of extended objects in the Bridge and one at the Small Magellanic Cloud wing tip might be currently forming dwarf spheroidal galaxies.
Revised and extended catalog Plate Plate designation --- Name Object name --- Cross-Id Cross-identifications --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Type Type number=1 C: star cluster A: association N: emission nebula --- Dmax Size of the major axis arcmin Dmin Size of the minor axis arcmin PA Position angle of the major axis (0deg=N, 90deg=E) deg Rem Remarks number=2 PN: planetary nebula mP: member of cluster pair mT: member of cluster triplet br*: a bright star is present att: attached to A hierarchical indication is given for objects embedded in or superimposed on larges ones: "in" suggests a possible connection, "sup" suggests a projection --- Excluded entries Name Name --- Rem Remarks --- N. G. Roman ADC/SSDOO - James Marcout, Patricia Bauer CDS 1997 Jun 12 UNKNOWN UNKNOWN A copy of table 2 was mailed by Eduardo L. D. Bica <bica@if.ufrgs.br> to Dr Nancy G. Roman in January 1997. Also prepared via OCR at CDS. Some corrections made in table2 on 14-May-1999 Versions merged on 20-Jun-1999. J_ApJS_101_41.xml The CNOC cluster redshift survey catalogs. II. Abell 2390. J/ApJS/102/289 J/ApJS/102/289 CNOC cluster redshift survey catalogs. II. The CNOC cluster redshift survey catalogs. II. Abell 2390. H K C Yee E Ellingson R G Abraham P Gravel R G Carlberg T A Smecker-Hane D Schade M Rigler Astrophys. J. Suppl. Ser. 102 289 1996 1996ApJS..102..289Y Clusters, galaxy Galaxy catalogs Redshifts catalogs galaxies: clusters: individual (A2390) galaxies: distances and redshifts galaxies: photometry A photometric and redshift catalog of galaxies in the field of the rich galaxy cluster Abell 2390 (z=0.228) is presented as part of the CNOC cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. Using five separate fields, the imaging and spectroscopic observations cover a strip of approximately 7.3'x43.2', centered on the cluster. Redshifts for 327 galaxies, primarily ranging in magnitude from r=17 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, geometric, and color selection functions for the redshift sample are discussed and presented.
ACO 2390 21 53.6 +17 40
Abell 2390 catalog PPP Object number number=1 The identification number is made of: - The first digit denotes the field of origin for the galaxy with the numbers 1, 2, 3, 4, and 5 representing the central, east 1, west 1, east 2 and west 2 field, respectively. - The second digit indicates whether the object is observed in one field or in an overlapping area from two fields. In the former, the second digit is 0; and in the latter, the second digit represents the field number of the overlapping field. - The last four digits denote the object number for each object within its own field, starting from the southern edge of the field, increasing to the north. --- oRA Offset in right ascension number=2 Offset from the first rank galaxy (positive is east and north). arcsec oDE Offset in declination number=2 Offset from the first rank galaxy (positive is east and north). arcsec rmag r magnitude mag g-r g-r color index mag z Heliocentric redshift --- e_z rms uncertainty on z 10-5 R Correlation significance parameter --- Class Spectral classification of object number=3 the classification is: 1 and 2: elliptical 3: E+A 4: Sbc 5: emission-line (Irr) 6: active galactic nucleus/ quasar 77: star 99: observed spectroscopically but no redshift obtained --- Wm Magnitude selection weight --- Wxy Geometric selection weight --- table2.tex LaTeX version of table2 Patricia Bauer CDS 1996 Aug 14 Howard Yee <hyee@cfht.hawaii.edu> J_ApJS_102_289.xml Extragalactic globular clusters. IV. The data. J/ApJS/102/29 J/ApJS/102/29 Extragalactic globular clusters Extragalactic globular clusters. IV. The data. J P Huchra J P Brodie N Caldwell C Christian R Schommer Astrophys. J. Suppl. Ser. 102 29 1996 1996ApJS..102...29H Clusters, globular Spectrophotometry galaxies: stellar content globular clusters: general stars, absundances This is a collection of line indices in the Lick system (and others) for a collection of Galactic, M31, M33 and other globular clusters plus bright and dwarf galaxies observed primarily at the MMT over the period 1980-1992 by J. Huchra, J. Brodie, N. Caldwell, R. Schommer, C. Christian and G. Bothun. The paper describing this catalog of indices is published in Huchra, Harris & Schommer (1996, in prep). Table 1 lists the definition of the indices used, Table 2 lists the line indices and errors, Table 3 lists multiple measurements for individual objects (plus dispersions and means) to give the reader a sense of the precision and accuracy of individual measures, and Table 4 lists index measurements from higher dispersion spectra. Each of the index tables generally has two lines, the first are the index values and the second are the statistical (calculated from photon counts) errors. An estimate of the external error in each index can be gotten from the multiple measurements given in Table 3. "AV" in Table 2 indicates that the measurement given is the average of multiple individual spectra give in Table 3. Otherwise the "RFN" number refers to the serial number of the MMT spectrum.
Definitions for line indices and colors n_Index Origin of the index number=1 S: Suntzeff Indices, 1980AJ.....85..408S and 1981ApJS...47....1S F: Faber and Burstein Indices, 1984ApJ...287..586B B: Brodie and Hanes Indices, 1986ApJ...300..258B C1 + C2 are the continuum bandpasses on either side of I the index bandpass --- Index Index name --- C1 Bandpass defined the C1 index --- I Bandpass defined the I index --- C2 Bandpass defined the C2 index --- Line indices and errors Multiple measurements, dispersion and errors Average dispersion and errors Gal Parent galaxy (only in table2) number=1 1: Andromeda Globular Cluster. Nomenclature for the Andromeda clusters follows Huchra et al., (1982ApJ...259L..57H), with the Battistini et al., (1980A&AS...42..357B), number first followed by the Sargent et al., (1977AJ.....82..947S), number. 2: M81 Globular Clusters 3: Fornax Dwarf Galaxy Globular Clusters 4: M33 Globular Cluster Candidates 5: M87 Globular Clusters 6: Virgo Dwarf Galaxies 7: Fornax Cluster Dwarf Galaxies 8: Other Dwarf Galaxies 9: Bright Galaxies. Several of the M31 cluster candidates have been classified as foreground stars (see Huchra et al., (1991ApJ...370..495H) for a discussion and complete identifications). Theses stars can be found in the "Other Stars" (13) section. 10: Peculiar Galaxies 11: Comparison Stars 12: Cluster System Averages. N188 AV is the weighted average of the individual NGC 188 stars. 13: Other Stars Individual notes: Dwarf galaxy identifications: Virgo dwarfs from Binggeli et al., (1985AJ.....90.1681B), and Caldwell, (1983AJ.....88..804C), as follows. N4472DW3 = VCC 1311 ; N4472DW10 = VCC 1435 ; N4472DW8 = VCC 1254 ; N4472DW1 = VCC 1107 ; M87DW6 = VCC 1407 ; N4472DW6 = VCC 1049 ; 1240+10 = VCC 1936? ; M87DW8 = VCC 1389 ; M87DW7 = VCC 1185 ; 1157+14 = dwarf near Virgo at 11h56m59.9s +14deg10'01". Identifications for individual stars are as follows. M2 stars = M2-68, M2-45 M3 stars = 3I-87, 3III-77, 3IV-25, 3III-28, 3-AV M5 stars = 5IV-86, 5III-3, 5IV-19, 5II-51, 5IV-59 M71 stars = A7, A6 NGC188 stars = II-51, II-76, II-88, I-57, I-1, II-72 M92 stars = VII-18, XI-19, XII-34, III-13, 92II-70, IV 114, IX-12, XII-18 M13 stars = 13-171, 13-786, 13-818, II-76, II-67 M15 stars = II-30, II-64, II-75 Draco stars = D-536, D-49, D-24,D-490, D-119, D-581, D-343, D361, D-45 Identification for "Other" stars are as follows. M87 GC candidates = III-151, I-84, III-239, 87-1535, III-200, 87-950, 87-874, 87-93, III-196, II-189 and II-93 M31 GC candidates = 000-000, 000-003, 000-13, 000-017, 000-320, GS-1 N147A = superposed bright star on NGC 147 AC211 = UV bright X-ray source candidate in M15 M49 GC candidates = C205, C153 and C279 Stars are grouped by parent star cluster or dwarf galaxy. --- Name Object name --- RFN Identification number from the MMT spectra number=2 RFN = reduced file number, except in table2, where AV indicates that entry is the signal-to-noise ratio --- CNB CNB index --- e_CNB rms uncertainty on CNB index --- CAs CAs index --- e_CAs rms uncertainty on CAs index --- H+K H+K index --- e_H+K rms uncertainty on H+K index --- Delta Delta index --- e_Delta rms uncertainty on Delta index --- CNR CNR index --- e_CNR rms uncertainty on CNR index --- CH CH index --- e_CH rms uncertainty on CH index --- Hbeta Hbeta index --- e_Hbeta rms uncertainty on Hbeta index --- MgH MgH index --- e_MgH rms uncertainty on MgH index --- Mg2 Mg2 index --- e_Mg2 rms uncertainty on Mg2 index --- Mgb Mgb index --- e_Mgb rms uncertainty on Mgb index --- MgG MgG index --- e_MgG rms uncertainty on MgG index --- Fe5270 Fe5270 index --- e_Fe5270 rms uncertainty on Fe5270 index number=3 In table2, line 193 (5 II-105 3049), e_Fe5270=-.157 in the printed table --- NaI NaI index --- e_NaI rms uncertainty on NaI index --- Line indices from high dispersion spectra Name Object name --- RFN Identification number from the MMT spectra --- CNR CNR index --- e_CNR rms uncertainty on CNR --- Hbeta Hbeta index --- e_Hbeta rms uncertainty on Hbeta --- CH CH index --- e_CH rms uncertainty on CH --- Mgb Mgb index --- e_Mgb rms uncertainty on Mgb --- CNB CNB index --- e_CNB rms uncertainty on CNB --- HK HK index --- e_HK rms uncertainty on HK --- DELTA DELTA index --- e_DELTA rms uncertainty on DELTA --- MgG MgG index --- e_MgG rms uncertainty on MgG --- Patricia Bauer CDS 1997 Mar 06 J. Huchra, Smithsonian Astrophysical Observatory J_ApJS_102_29.xml ROSAT Observations of the Pleiades. I. X-Ray Characteristics of a Coeval Stellar Population J/ApJS/102/75 J/ApJS/102/75 ROSAT Observations of the Pleiades ROSAT Observations of the Pleiades. I. X-Ray Characteristics of a Coeval Stellar Population G Micela S Sciortino V Kashyap F R Harnden R Rosner Astrophys. J. Suppl. 102 75 1996 1996ApJS..102...75M I/90 : Positions of 502 Stars in Pleiades Region (Eichhorn+ 1970) I/163 : US Naval Observatory Pleiades Catalog (Van Flandern 1969) Clusters, open Rotational velocities X-ray sources Of 214 stars in the core of the Pleiades, 99 were detected in X-rays with the ROSAT PSPC. This catalog lists the characteristics of the stars taken from the literature, in table1.dat and the rotational and X-ray characteristics in table5.dat.
The nucleus of the composite catalog used in this study is the catalog compiled from the published literature for the Einstein investigations of the Pleiades (Micela et al. 1990). This list has been extended by the results of recent surveys to a completeness limit of visual magnitude about 18. ROSAT
Basic data ID Micela number --- name Name --- RAh Right Ascension hours (J2000) h RAm Right Ascension minutes (J2000) min RAs Right Ascension seconds (J2000) s DE- Declination sign (J2000) --- DEd Declination degrees (J2000) deg DEm Declination minutes (J2000) arcmin DEs Declination seconds (J2000) arcsec Vmag V magnitude mag r_Vmag Reference for Vmag --- B-V B-V color mag Sp Spectral type --- r_Sp Reference for spectral type --- l_vsini < indicates upper limit for vsin(i) --- vsini Rotation velocity * sin(inclination) From Soderblom et al. (1993ApJS...85..315S; Cat. <J/ApJS/85/315>) km/s rem Notes --- r_vsini Reference --- Rotation and X-ray characteristics ID Micela number --- rem "*" indicates E(B-V) > 0.1 --- name Name --- oRA Difference in right ascension The difference between the position derived from the ROSAT image and the catalog position of the suggested identification for sources not in complexes of overlapping sources. s oDE Difference in declination arcsec off_axis Off axis value The spatial resolution of ROSAT degrades with distance from the axis. The accuracy radius for identification is taken as 30" sources within 20' of the axis and 60" for sources between 30' and 50'. Sources beyond 50' from the axis were not included. arcmin l_CtRate < indicates upper limit for CtRate --- CtRate Count rate ct/ks S/N Signal/noise ratio --- HR Hardness ratio HR = (counts(0.2-0.9 keV))/(counts(0.9-2.01 keV)) --- e_HR Mean error on HR --- cecf Counts-to-energy conversion factor 10-14W/ct l_log_Lx < indicates upper limit for log(Lx) --- log_Lx Log of X-ray luminosity Computed for assumed distance of 127 pc. 10-7W mcpt Multiple counterparts Numbers indicate sources identified with more than one star or un complexes of overlapping sources. Stars with the same number are identified with the same X-ray source. --- References RefNo Reference number --- Text Text of reference, starting by the bibcode --- N. G. Roman ADC/SSDOO 1997, rev. F. Ochsenbein [CDS] 18-Jul-1998 Feb 21 J_ApJS_102_75.xml An infrared spectral atlas of Arcturus for the range 10750-11500cm-1 (8690-9300A) J/ApJS/103/235 J/ApJS/103/235 Arcturus IR spectral atlas An infrared spectral atlas of Arcturus for the range 10750-11500cm-1 (8690-9300A) L Wallace K Hinkle Astrophys. J. Suppl. Ser. 103 235 1996 1996ApJS..103..235W J/PASP/107/1042 : Infrared Arcturus Atlas (Hinkle+ 1995) Spectra, infrared Stars, variable infrared: stars line: identification stars: individual (Alpha Boo) An atlas of Arcturus spectra is presented spanning the 8690-9300A (10750-11500cm^-1^) region. The high-resolution (lambda/delta(lambda)~56000) Fourier transform spectra have been divided by a transmission function for the Earth's atmosphere. The Arcturus spectral features have been identified. This spectral region spans a gap between two major atlases, and comparison of the atlases is undertaken. The influence of a grating spectrograph's instrumental profile on equivalent width as well as line depth is noted. There is an overlap of 10cm-1 between the atlas profiles.
Arcturus HD 124897 HR 5340 14 15 43.5 +19 12 37
Spectral atlas for wavenumber 10750 Spectral atlas for wavenumber 10850 Spectral atlas for wavenumber 10950 Spectral atlas for wavenumber 11050 Spectral atlas for wavenumber 11150 Spectral atlas for wavenumber 11250 Spectral atlas for wavenumber 11350 Spectral atlas for wavenumber 11450 Freq Frequency scale in wavenumbers cm-1 Obs Derippled, observed Arcturus spectrum (removal of residual fringing) number=1 These data are in intensity units normalized to highest point. --- Telluric Telluric spectrum (used on the observed spectrum) number=1 These data are in intensity units normalized to highest point. --- Rat Ratioed spectrum after smoothing and continuum adjustment number=1 These data are in intensity units normalized to highest point. --- Line list Freq Frequency in wavenumbers cm-1 Ident Line identification --- CDS 1996 Sep 06 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 23-Apr-96 J_ApJS_103_235.xml Radio properties and optical identification of two samples of milliJansky radio sources at 1.4 GHz J/ApJS/103/331 J/ApJS/103/331 mJy radio sources at 1.4 GHz Radio properties and optical identification of two samples of milliJansky radio sources at 1.4 GHz N Y Lu G L Hoffman E E Salpeter J R Houck Astrophys. J. Suppl. Ser. 103 331 1996 1996ApJS..103..331L J/AJ/99/1071 : 1.4 GHz source survey (Condon+ 1990) Galaxies, radio Morphology Photometry Radio lines galaxies: distances and redshifts galaxies: photometry galaxies: structure radio continuum: galaxies surveys From the 1.4GHz radio survey of Condon, Dickey, & Salpeter (Cat. <J/AJ/99/1071>) in a region much devoid of rich galaxy clusters at redshifts z<0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}>11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R>20mag, suggesting that these are probably distant (z>0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}>5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R<15, the sample is dominated by elliptical galaxies with 16<R<18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R<17mag (z<0.2) to that of galaxy groups to clusters at R>18mag (z>0.3) .
Results from the radio-continuum snapshot observations at 4.86GHz. Name Source name --- n_Name n for near --- Note Note on radio signal number=1 a: Radio signals are weak b: Radio signals are weak. Only the two largest components are listed, i.e. the one on the most left and the one in the middle of the radio contour plot in Fig. 2 c: Radio signals are weak. Two components of R203 are shown separatedly in Fig. 2 as R203A and R203B. The objects are at the center of each plot d: Not detected. Upper limits are 3{sigma} --- RAh Right ascension (1950) number=2 Peak position of the best-fit Gaussian profile to each signal h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec l_Smax Limit flag on Smax --- Smax Peak flux density mJy e_Smax rms uncertainty on Smax mJy l_S4.86GHz Limit flag on S4.86GHz --- S4.86GHz Integrated flux density at 4.86GHz mJy e_S4.86GHz rms uncertainty on S4.86GHz mJy l_2a Limit flag on 2a --- 2a Estimated major axis arcsec e_2a rms uncertainty on 2a arcsec l_2b Limit flag on 2b --- 2b Estimated minor axis arcsec e_2b rms uncertainty on 2b arcsec PA Position angle (north to east of major axis) deg e_PA rms uncertainty on PA deg Radio properties of sample sources at 1.4 and 4.86GHz Name Source name --- m_Name Multiplicity index on Name --- n_Name Note on Name number=1 a: Not observed at 4.86 GHz --- Sample Sample number=2 DS: Distant sample NS: Nearby sample a: additional source --- RAh Right ascension (1950) number=3 Position of the adopted center of the source h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec S1.4GHz Integreted flux density at 1.4GHz mJy l_S4.86GHz Limit flag on S4.86GHz --- S4.86GHz Integreted flux density at 4.86GHz mJy SI Spectral index between 1.4 and 4.86GHz --- l_theta Limit flag on theta --- theta (maximum) angular size from 4.86GHz radio map arcsec PA Position angle (north to east) number=4 Positon angle of the major axis fro single component sources or of the axis connecting the two radio lobes for double-lobed sources deg Morph Morphology --- Results from the R-Band CCD imaging photometry Name Source name --- m_Name Multiplicity index on Name --- n_Name Note on Name number=1 a: The optical counterpart lies slightly outside the error ellipse. It was accepted, for it is either optically bright with a radius much larger than its apparent angular distance to the radio source position or well between the two radio lobes. b: The integration time for the R-band CCD image is only 300s. c: R082 is in a very dense galaxy cluster at z=4.407 (Dressler & Gunn 1992, Cat. <J/ApJS/78/1>). The magnitude may be slightly contaminated. d: There is an optical object near one of the radio components. e: This optical identification is slightly outside the error ellipse. It was accepted because the central position of this weak radio source is somewhat uncertain. f: Radio map at 4.86 GHz is not available. The offsets (i.e., cols. [oRAr] and [oDEr]) for the second probable optical counterpart are with respect to the optical position of the first one. --- Date Observation date "DD/MM/YY" FWHM FWHM of the optical seeing arcsec Nopt Number of the detected optical object with R<23.5mag --- a Semi-major axis arcsec --- --- b Semi-minor axis arcsec PA Position angle (North to East) deg oRAr Positional offset in RA direction, from the radio position to the position of an optical identification arcsec oDEr Positional offset in DE direction, from the radio position to the position of an optical identification arcsec oRAs Offset in RA direction, from a nearby bright star to the optical identification arcsec oDEs Offset in DE direction, from a nearby bright star to the optical identification arcsec l_Rmags Limit flag on Rmas --- Rmags R magnitude of the offsetting star mag n_Rmag B: bright --- Type Type (Gal or QSO) --- Rmag FOCAS-measured isophotal magnitude mag Aiso Isophotal area arcsec+2 2a Major diameter of optical identification arcsec --- --- 2b Minor diameter of optical identification arcsec PAo Position angle of the optical identification (North to east) deg James Marcout, Patricia Bauer CDS 1998 Apr 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_103_331.xml A catalog of candidate field horizontal-branch and A-type stars. II. J/ApJS/103/433 J/ApJS/103/433 Horizontal-branch and A-type star catalog. II A catalog of candidate field horizontal-branch and A-type stars. II. T C Beers R Wilhelm S P Doinidis C J Mattson Astrophys. J. Suppl. Ser. 103 433 1996 1996ApJS..103..433B Stars, A-type Stars, horizontal branch catalogs stars: horizontal-branch We present coordinates and brightness estimates for 4175 candidate field horizontal-branch and A-type stars, in the magnitude range 10<=B<=15.5, selected using an objective-prism/interference-filter survey technique. The candidates lie primarily in the northern Galactic hemisphere and complement a previously published sample of southern Galactic hemisphere candidates. Available spectroscopy and photometry indicates that the great majority of the candidates are likely to be bona fide members of either the field blue horizontal- branch population or the blue, metal-deficient, high surface gravity stars referred to by Preston, Beers, & Schectman (1994AJ....108..538P) as BMP stars. The remaining stars in the catalog are likely to be a mix of metal-deficient turnoff stars, metallic-line (Am) stars, field red horizontal-branch stars, optical doubles with overlapping objective-prism spectra, and (particularly among the fainter candidates) inadvertently included late-type stars.
Candidate Field Horizontal-Branch and A-Type Stars Plate Plate ID A 5-digit integer indicating the Burrell Schmidt HK objective-prism/interference-filter plate number on which the star is located. --- Star Star number on the Plate --- Class Classification, A or AB --- Bright Brightness classification Seven brightness classes are used: very bright (vb), bright (b), medium bright (mb), medium (m), medium faint (mf), faint (f), and very faint (vf). Stars which are judged to be ideally exposed are grouped into brightness class m; stars brighter or fainter than the ideal case are divided into the remaining classes. As a result, the true apparent magnitudes of the catalog stars within any brightness class will vary somewhat from plate to plate. --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec GLAT Galactic latitude deg GLON Galactic longitude deg CDS 1996 Sep 06 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 03-May-96 J_ApJS_103_433.xml Far-ultraviolet stellar photometry: fields centered on Rho Ophiuchi and the Galactic center J/ApJS/104/101 J/ApJS/104/101 Far-UV stellar photometry Far-ultraviolet stellar photometry: fields centered on Rho Ophiuchi and the Galactic center E G Schmidt G R Carruthers Astrophys. J. Suppl. Ser. 104 101 1996 1996ApJS..104..101S Photometry, ultraviolet Galaxy: center ISM: individual (Rho Oph) stars: fundamental parameters surveys ultraviolet: stars Far-ultraviolet photometry is presented for 121 objects in a 20deg diameter field centered on Rho Oph and for 649 objects in a field covering the Galactic center. Broadband magnitudes with effective wavelengths of 1375A and 1781A are given. The Galactic center field overlaps two fields which were discussed in an earlier paper. Eighty- eight percent of the ultraviolet objects in the Rho Oph field were identified with visible stars using the SIMBAD database, while only 9% of the objects are blends of early-type stars too close together to separate with our resolution. The photometric calibration was studied in detail, and corrections for nonlinearity were derived for the fields analyzed earlier as well as those discussed here. For stars in common between the Galactic center field and the previous fields, a comparison of the magnitudes yielded estimates of the internal errors of the magnitudes of sigma_1375=0.13mag and sigma_1781=0.21mag. A collated list of stars in the fields covering the Galactic center and incorporating the revised calibration is presented and compared with the S201 data of the same region. The properties of the sample of ultraviolet objects in the Rho Oph field are briefly commented upon.
Ultraviolet objects in the rho Ophiuchi field Ultraviolet objects in the galactic center field Collated list of objects from the Scorpius, Sagittarius, and Galactic center fields Star Star number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin m1375 137.5mm UV magnitude mag m1781 178.1mm UV magnitude mag OptID Optical identification --- n_OptID Note on Ident number=1 In table2 A : There are five B stars within a few arcminutes of the ultraviolet object in addition to HD 145502. However, all are of spectral type B8 or B9 (as compared with B2 for HD 145502) and are fainter. Hence, HD 145502 should be the source of most of the ultraviolet flux. B : The ultraviolet source is the hot, main-sequence companion of Alpha Sco. In table3 a: This object is an unresolved clump of star in the cluster Bochum 13 b: This object is an unresolved clump of stars in the cluster NGC 6383. The magnitude and spectrum refer to the brightest star, HD 159176, which should dominate the ultraviolet flux. c: These objects are unresolved clumps of stars in the cluster NGC 6405 d: These objects are unresolved clumps of stars in the cluster NGC 6475 e: These objects are unresolved clumps of stars in the cluster NGC 6530 f: This object consists of a number of stars in the cluster NGC 6530, but the ultraviolet is likely to be dominated by HD 164794 and NGC 6530-9. The V magnitude is a combination of those two stars. g: This object is an unresolved clump of stars in the cluster NGC 6531 h: This object is an unresolved group of stars in the cluster Colinder 367. The magnitude and spectrum refer to HD 165921, which should dominate the ultraviolet flux --- Vmag Visual or photographic magnitude mag n_Vmag P if Vmag is a photographic magnitude --- V-B V-B color mag Sp Spectral type --- table5.fit FITS ASCII table version of table5 CDS 1996 Sep 06 Table 5 from AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 03-May-96 Table 2 and table 3 prepared via OCR at CDS [CDS] 17-Jun-97 UNKNOWN UNKNOWN Table2 and Table3 added on 17 Jun 1997 J_ApJS_104_101.xml Ultraviolet imaging telescope near-ultraviolet bright object catalog. J/ApJS/104/287 J/ApJS/104/287 UIT near-UV bright objects catalog Ultraviolet imaging telescope near-ultraviolet bright object catalog. E P Smith A J Pica R C Bohlin R H Cornett M N Fanelli W B Landsman R W O'Connell M S Roberts A M Smith T P Stecher Astrophys. J. Suppl. Ser. 104 287 1996 1996ApJS..104..287S Photometry, ultraviolet catalogs galaxies: photometry ultraviolet: stars We present a photometric catalog of 2244 objects detected by the Ultraviolet Imaging Telescope in the near-ultraviolet (NUV; 1650A<lambda<2900A) during the Astro-1 Space Shuttle mission. Sources in the catalog are as faint as m_nuv~18.8, or f_nuv~1.1x10^-16ergs/s/cm^2/A, but the survey is not complete to this level. Optical catalogs were used to cross identify sources and derive NUV-V colors. A majority of the objects (88%) do indeed have proposed optical identifications from catalogs, and most are stars. Our purpose in creating the catalog is to form a database useful for identifying very blue objects and performing Galactic UV stellar population studies.
ASTRO 1/UIT
UIT pointings in catalog RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Target UIT target --- Exp Longest exposure time & assoc. frame number s Filter UIT filter A5 and A2 data represent orbital day exposures --- Frame Associated UIT frame number --- UIT near-UV bright object catalog Entry Catalog entry number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec mnuv Near-UV aperture magnitude mag n_mnuv Flag for stars w/ saturated pixels --- e_mnuv Uncertainty in mnuv mag mnuv-V mnuv - V color mag Type Object classification The object is classified with a two-digit number. The first digit represents the UIT filter used for the observation, while the second digit represents the type of optical identification. A "0" represents a cataloged stellar identification (either named or from the HST GSC), a "1" indicates a nonstellar source, and a "2" indicates a proposed match with the digitized POSS (265 sources). --- Name Name, if any, of the ID, or a brief note Most of the objects (second classification digit "0") match stars from the HST GSC, and no name is listed for these objects. --- Frame UIT frame number used for the photometry --- table1.tex AASTeX version of table1.dat table2.tex AASTeX version of table2.dat CDS 1997 Feb 10 Eric P. Smith esmith@hubble.gsfc.nasa.gov AAS CD-ROM Vol.7 Lee Brotzman [ADS] 16-Jul-96 J_ApJS_104_287.xml UBV photometry of OB associations within superbubbles of the Large Magellanic Cloud J/ApJS/104/71 J/ApJS/104/71 UBV photometry of OB associations in LMC superbubbles UBV photometry of OB associations within superbubbles of the Large Magellanic Cloud M S Oey Astrophys. J. Suppl. Ser. 104 71 1996 1996ApJS..104...71O H II regions Magellanic Clouds Nebulae Photometry, UBV HII regions ISM: bubbles Magellanic Clouds open clusters and associations: general Tables 4a-m provide the photometry for the OB associations of the sample, including both superbubbles and diffuse H II regions. Notes for individual objects are: DEM 31: Photometry for D31-2001 (Sk -67 17) listed from Ardeberg et al. (1972A&AS....6..249A) DEM 106: Stars with prefix D106A- have V photometry from a separate, short exposure. DEM 192: Stars with prefix D192A- have V photometry from a separate, short exposure. DEM 301: Photometry for D301-1005 listed from Massey et al. (1995ApJ...438..188M) Postscript versions of the plates in Figure 1 of the printed paper are included. Each is a V image of the OB association field, with bright stars identified. The remaining stars can be identified with the aid of coordinates given in Table 4a-m. Each individual frame is 3.8' x 3.8' square, with north up and east to the left. This work presents UBV photometry of the stellar populations associated with seven superbubble nebulae and five classical H II regions in the Large Magellanic Cloud. Although the nebular morphology of the superbubbles appears to be substantially evolved compared to the classical nebulae, the color-magnitude diagrams do not reveal any noticeable correlation between the resident stellar population and nebular morphology. The photometry presented here will be used in a forthcoming paper to examine further the stellar content and dynamics of these superbubbles.
Photometry for DEM 25 Photometry for DEM 31 Photometry for DEM 50 Photometry for DEM 106 Photometry for DEM 192 Photometry for DEM 226 Photometry for DEM 231 Photometry for DEM 301 Photometry for DEM 10b Photometry for DEM 66 Photometry for DEM 197 Photometry for DEM 243 Photometry for DEM 293 ID Star identification Star identification. Stars with a and b components are spectroscopic binaries, whose V magnitude has been estimated as described in the printed paper. However, the colors listed for both components are the original, combined colors determined for the composite object. The DAOPHOT errors for these objects are misleading, and have been deleted. --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec Vmag V magnitude mag e_Vmag Error in Vmag These are the photometric errors computed by DAOPHOT and do not include systematic effects such as those introduced by aperture corrections and transformation errors. mag B-V B-V color mag e_B-V Error in B-V mag U-B U-B color mag e_U-B Error in U-B mag figure1a.ps V image for DEM 25 figure1b.ps V image for DEM 31 figure1c.ps V image for DEM 50 figure1d.ps V image for DEM 106 figure1e.ps V image for DEM 192 figure1f.ps V image for DEM 226 figure1g.ps V image for DEM 231 figure1h.ps V image for DEM 301 figure1i.ps V image for DEM 10b figure1j.ps V image for DEM 66 figure1k.ps V image for DEM 197 figure1l.ps V image for DEM 243 figure1m.ps V image for DEM 293 CDS 1996 Sep 06 AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 03-May-96 J_ApJS_104_71.xml Low surface brightness galaxies in the local universe. I. The catalog. J/ApJS/105/209 J/ApJS/105/209 Low surface brightness galaxies. I. The catalog Low surface brightness galaxies in the local universe. I. The catalog. C D Impey D Sprayberry M J Irwin G D Bothun Astrophys. J. Suppl. Ser. 105 209 1996 1996ApJS..105..209I J/ApJ/463/535 : 1996ApJ...463..535S : Paper II. Sprayberry et al. (Paper III in prep.) Galaxies, photometry galaxies: distances and redshifts galaxies: fundamental parameters galaxies: luminosity function, mass function galaxies: photometry radio lines: galaxies surveys Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z<=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.
Low Surface Brightness (LSB) Galaxies, Large Angular Size LSB Galaxies, Small Angular Size Name Galaxy name --- n_Name Note number=1 c: Object with name ending in `x' not identified in original scan of UKST plates, but included because it could be observed simultaneously with identified object nearby. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec HRV Heliocentric radial velocity determined from the low-resolution optical spectroscopy for galaxies observed with the MMT km/s HRVHI Heliocentric radial velocity determined from the radio observations for galaxies detected in 21cm HI emission km/s Btot Total B magnitude mag mu0 Central surface brightness in B magnitude mag/arcsec2 mue Surface brightness in B magnitude at the effective radius mag/arcsec2 Reff Effective radius arcsec log(MHI) HI mass solMass BMag Absolute B magnitude mag Com Comments number=2 Explanation of the `Comments' column: 1) the first entry for each galaxy is its Hubble type, with `cpn' used as an abbreviation for `companion' where appropriate 2) for galaxies described as `Interacting', the radio and optical luminosities include the complete interacting system, unless indicated otherwise; 3) the entry `CCD' indicates that the magnitudes were obtained from direct CCD observations, and the absence of such an entry indicates that the magnitudes were obtained from the APM scans of the UK Schmidt survey plates 4) the entry `H I n/d' indicates that the galaxy was observed but not detected in the 21 cm line redshifted to the radial velocity determined from optical spectroscopy 5) the entry `Vopt?' indicates that the optical spectrum has a very low S/N ratio and that the radial velocity determined from that spectrum is therefore unreliable 6) the entry `delta_v cpn' indicates that a large difference between V_opt and V_HI is probably due to dynamical interaction with a companion. Notes (preceded by ^): a) Reduced photometric accuracy due to light clouds. b) Putative detection may be GPS satellite or other interference. d) No detection at known radial velocity, but severity of interference prevents determination of a meaningful upper limit on gas mass. e) Obvious detection, but interference prevents accurate measurement of flux integral; reported gas mass is a lower limit. f) Reduced photometric accuracy due to scattered light or other instrumental problem. --- LSB Galaxies: Catalog Cross-Identifications Name Galaxy name from table1 or table2 --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec ID Catalogue designation --- RAh2 Right ascension (1950) h RAm2 Right ascension (1950) min RAs2 Right ascension (1950) s DE-2 Declination sign --- DEd2 Declination (1950) deg DEm2 Declination (1950) arcmin DEs2 Declination (1950) arcsec Patricia Bauer CDS 1997 Feb 21 Thanks are due to H. Andernach <hja@hja.vilspa.esa.es> who forwarded his copy (catalog numbered A321 in his list) originally mailed in latex by Chris Impey <impey@as.arizona.edu> J_ApJS_105_209.xml Galactic H I column densities toward quasars and active galactic nuclei J/ApJS/105/369 J/ApJS/105/369 Galactic H I column densities Galactic H I column densities toward quasars and active galactic nuclei E M Murphy F J Lockman A Laor M Elvis Astrophys. J. Suppl. Ser. 105 369 1996 1996ApJS..105..369M Active gal. nuclei H I data QSOs Galaxy: structure radio lines: ISM X-rays: general The file data.fit contains the data for all 220 objects as FITS IMAGE extensions. The spectrum for each object is written as an image extension in the same order as printed in table 1 (and the FITS table in the first file). The data are written as 1-dimensional spectra and are in units of brightness temperature in Kelvins. In the header, the LSR velocity (CRVAL1), the reference pixel (CRPIX1), and the velocity increment (CRPIX1) can by used to calculate the LSR velocity of a given pixel. Note that the data are linear in frequency, not velocity, and this must be taken into account when calculating the velocity of a given pixel. The FITS files were written using the CFITSIO package written by Dr. William Pence at the GSFC. We have determined accurate values of the Galactic neutral hydrogen column density, N_H_, toward 220 quasars and active galactic nuclei from 21cm H I measurements made on the 130 Foot Telescope (42.7m). Accurate values of N_H_ have now been obtained for the whole PG bright quasar sample and most quasars that have been observed by ROSAT and the Hubble Space Telescope through mid-1993. The spectra were corrected for stray 21cm radiation yielding values of N_H_ with a typical uncertainty of 1x10^19cm^-2 for high Galactic latitude directions. The H I column densities will be useful for correcting for interstellar opacity at UV and soft X-ray wavelengths, and for estimating the reddening and extinction toward these objects.
Summary of 21 cm H I observations Object Object name --- RAdeg Right ascension, 1950 deg DEdeg Declination, 1950 deg GLon Galactic longitude deg GLat Galactic latitude deg NH_Thin Optically thin H I column density cm-2 NH_TS150 Uniform temp 150 K H I column density cm-2 Comment Comment number 1) Data not corrected for stray radiation 2) The listed value of NH includes emission only between LSR velocities -60km/s and +28km/s. The H I in NGC 247 itself appears in the spectrum at V_LSR>+28km/s. --- Image Image extension number The image extension number of the data for each object in the data file, data.fit. --- data.fit FITS IMAGE Extension file of spectra CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 22-Oct-96 J_ApJS_105_369.xml A Moderate-Resolution Spectral Atlas of Carbon Stars: R, J, N, CH, and Barium Stars J/ApJS/105/419 J/ApJS/105/419 Moderate-Res Spectral Atlas of Carbon Stars A Moderate-Resolution Spectral Atlas of Carbon Stars: R, J, N, CH, and Barium Stars C Barnbaum R P S Stone P C Keenan Astrophys. J. Supp. 105 419 1996 1996ApJS..105..419B III/150 : Perkins Revised MK Types for the Cooler Stars (Keenan+ 1989) Barnbaum C., Stone R.P.S., and Keenan P.C. 1996, ApJS 105, 419 =1996ApJS..105..419B Keenan, P. C. 1993, PASP, 105, 905 =1993PASP..105..905K Keenan, P. C. and Morgan, W. W. 1941, ApJ, 94, 501 =1941ApJ....94..501K Spectra Spectral types Stars stars: carbon The authors compiled this moderate-resolution spectral atlas to aid in the classification of carbon stars on the Revised MK System (Keenan 1993) as refined and extended by the present work. Hence the main purpose of this atlas is to permit rapid and reasonably accurate comparison of the properties of carbon stars in the Solar neighborhood with those in the Galactic bulge, the Magellanic Clouds, and in other nearby external systems. The classification scheme employed makes no assumptions about evolutionary status of the stars but is based entirely on observable criteria. Spectra of 39 stars are presented in detail, along with a catalog of 119 carbon stars classified according to the Revised MK System. Included is a catalog of spectral types for 119 carbon stars classified according to the Revised MK scheme. The catalog lists the classification for each star, variability type (from Kholopov 1985), and instrument used.
Except for the early R stars, most carbon stars have spectra so densely occupied by bands of carbon compounds that nearly all the atomic lines that normally provide the criteria for spectral classification are either distorted or obliterated. It is this complexity that makes it so difficult to sort the spectra into types that can be calibrated in terms of fundamental physical variables: effective temperature (Teff), luminosity, and composition. Nevertheless, the authors have been able to assign temperature types, luminosity classes (at least for the R stars) and abundance indices for the principal compounds of carbon. The C2 index is included in the type for every carbon star; it seems to be the best measure of the ratio of carbon to oxygen. In using the index, allowance must be made for its sensitivity to temperature also. The C2 index runs from 1 to 5, indicating that the strong bands at 4737 and 5135 A are barely visible at the atlas scale. Other indices are included in the type only when it appears necessary to call attention to the behavior of a particular feature. Thus, for example, a CH index of 3.5 or greater defines a CH star. Since the relative strengths of the bands of carbon compounds containing the isotopes 12C and 13C differ widely in different kinds of carbon stars, an isotopic index, j, is used as a measure of 12C/13C. The index and its range from 1 to 5 agree with the usage of Yamashita (1972). Normally this index is included in the type only when j > 3.5 which defines an isotopic (or J) star. The relation of the index to isotopic ratio is shown in Table 1 of Barnbaum et al (1996). Notation, however, is not the only problem. Both theory and observation have made it clear that an excess of carbon over oxygen can appear in the atmospheres of stars of different masses or original composition at different stages of their evolution. The new classification attempts to assign different spectral types to members of different spectroscopic groups. The spectra: The spectral files are the data for the standard Carbon Stars in Figs 1 and 2 of Barnbaum et al. (1996).
AC Per low res spectrum AC Pup low res spectrum AQ And blue order AQ And red order AQ Sgr blue order AQ Sgr red order BD +2 3336 blue order BD +2 3336 red order BL Ori low res spectrum BL Gem low res spectrum CZ Mon low res spectrum DF Mon low res spectrum DY Per blue order DY Per red order EL Aur low res spectrum EU And blue order EU And red order </tableLink> <tableLink xlink:href="u_aurl.dat"> <title>U Aur low res spectrum GK Ori low res spectrum GY Mon low res spectrum HD 100764 echelle spectrum HD 10636 blue order HD 10636 red order HD 112127 echelle spectrum HD 113801 echelle spectrum HD 123821 echelle spectrum HD 156074 blue order HD 156074 red order HD 178717 blue order HD 178717 red order HD 182040 blue order HD 182040 red order HD 19557 blue order HD 19557 red order HD 198269 blue order HD 198269 red order HD 19881 blue order HD 19881 red order HD 199939 blue order HD 199939 red order HD 201657 blue order HD 201657 red order HD 209621 blue order HD 209621 red order HD 211594 blue order HD 11594 red order HD 217143 blue order HD 217143 red order HD 223392 blue order HD 223392 red order HD 223617 blue order HD 223617 red order HD 26 blue order HD 26 red order HD 5223 blue order HD 5223 red order HD 76396 low res spectrum HD 76846 echelle spectrum HO Cas blue order HO Cas red order NQ Cas blue order NQ Cas red order R Scl blue order R Scl red order RS Cyg echelle spectrum RT Ori low res spectrum RV Sct blue order RV Sct red order RY Hya low res spectrum S Aur low res spectrum S Sct blue order S Sct red order SS Vir low res spectrum SU And blue order SU And red order SZ Sgr blue order SZ Sgr red order T Cnc low res spectrum T Lyr echelle spectrum TT Tau low res spectrum TU Gem low res spectrum TU Tau low res spectrum TV Lac blue order TV Lac red order TW Oph blue order TW Oph red order TX Aur low res spectrum U Aur low res spectrum U Hya low res spectrum V1942 Sgr blue order V1942 Sgr red order V460 Cyg blue order V460 Cyg red order V Ari blue order V Ari red order VX And blue order VX And red order W Cma low res spectrum W Ori low res spectrum WX Cyg blue order WX Cyg red order X Cnc low res spectrum Y Cvn low res spectrum Y Tau low res spectrum Z Psc blue order Z Psc red order lambda wavelength in Angstroem 0.1nm flux relative or normalized flux --- Catalog of standard stars on the Revised MK System HD HD number --- HDsuffix HD suffix --- alt BD number or name --- Sp Spectral Classification: Type --- C2 Spectral Classification: C2 index --- OtherIdx Spectral Classification: Other index --- LClass Spectral Classification: Luminosity Class --- Var Var. (?) --- RAh Right Ascension (J2000) hours h RAm Right Ascension (J2000) minutes min RAs Right Ascension (J2000) seconds s DE- Declination (J2000) sign --- DEd Declination (J2000) degrees deg DEm Declination (J2000) arcmin arcmin notes Key to the notes a Instrument used for classification if not Kast or echelle on 1 m telescope: photographic plates taken at CTIO for the southern stars and at Lowell Observatory for the northern stars, all at similar resolution to the Kast spectra b Instrument used for classification if not Kast or echelle on 1 m telescope: Hamilton echelle spectrograph on the 3m telescope from the Barnbaum atlas c The spectral types for these stars have been slightly revised from those presented in Keenan 1993. d Special Notes: DY Per -- This star has shown sudden drops in brightness of the order of 3 magnitudes in several passbands. The type given here applies to normal maximum light. TW Hor = BS 917 = HD20234 -- This is Herschel's red star. TU Tau, FU Aur, GK Ori, CoD-262983, UU Aur, GY Mon, AC Pup, V901 Sco, SS Sgr -- No observations in the blue region. RT Pup -- a marginal J star. HD 100764 -- A peculiar star; see the description of the spectrum in Fig. 1a of Barnbaum et al. 1996 West 079-02: abbreviated ID for: Westerlund 079-02 -- This is the very red star seen by J. Herschel very close to b Cru. HD 148839 -- All spectral features very weak, as is generally true of C-Hd stars. This star also has a high velocity. V460 Cyg = HD 206570 = BS 8297 -- In older catalogs designated as DS Peg. EU And, BM Gem, and V778 Cyg -- carbon stars with oxygen-rich dust. The Spectral Classes (Extract from the source reference): R Stars: Type C-R --- These are the warmest of the carbon stars, with the exception of a few early CH stars. For most of them, the blue region is accessible to observation, and atmospheric analyses have shown that they have nearly solar abundances of the s-process elements. Hence, the usual ratios (Sr II blend 4077/Fe 4063, 4071 and Fe, Y II 4376/Fe 4383) can be used to assign luminosity classes. J Stars: Type C-J--- Spectroscopic criteria for identifying J stars are conspicuous enough to justify their being assigned to a different spectral class. In the blue region the 12C13C band at 4752 can be clearly seen even at rather low-resolution. For the red region Gordon (1967) defined a J star as one in which the strength of the 6168 C2 band is half the strength of 6122, and we assign isotopic indices of j=4.5 or greater to the J stars from this ratio and that of the CN bands at 6260 and 6206. (This corresponds to a range of 12C/13C from a bout 2 to 6.) The J stars include most of the stars that had been called either late R stars or early N stars in various catalogs and were provisionally assigned to the class C-RN by Keenan (1993). N stars: Type C-N--- These are the best known carbon stars and the ones most easily detected in infrared surveys. They are usually recognized by their extreme redness with a strong blue depression often nearly obliterating the spectrum below 4400 A. The isotopic bands are consistently weak, while lines of s-process elements, particularly Ba, are more enhanced than in R stars. The range of 12C/13C in N stars is usually from 30 to 70. Hydrogen-Deficient Carbon Stars: Type C-Hd--- We have classified here only the rare C-Hd stars that have nearly constant light (3 stars in Table 4) and have omitted R CrB variables whose spectra, like Miras, originate in different levels of their atmosphere depending on phase. The C-Hd stars are easily recognized; their spectral features resemble those of late G-type supergiants of luminosity class Ib except for the presence of CN and C2 and the almost complete absence of the G-band of CH and the lines of hydrogen. It is unclear whether the weakly variable C-Hd stars are R CrB variables at some other period of their history, or whether the two groups follow different evolutionary paths. CH Stars: Type C-H--- CH stars have long been recognized as Population II analogues of the R stars. Their range of temperatures is similar, but their distribution and high space motions relative to the sun place most of them in the Galactic halo. Spectroscopically, they are recognized by the dominance of CH bands in the blue region. Care must be taken, however, not to rely on the strength of the G-band alone, for, in an early carbon star with abundant carbon, it is nearly saturated. More useful are the secondary P-branch head near 4342 A and the weakening of features such as Ca 4226 by the network of faint bands of the same system. Barium Stars: Type Ba--- These are generally of temperature sequence G8 to K2 with the ionic lines of Ba, Sr, and Y greatly enhanced in their spectra, and for that very reason it is difficult to assign individual spectroscopic absolute magnitudes to them. Analyses of the high-resolution spectrograms, however, are most consistent with a giant luminosity. They probably have a considerable spread in luminosities, and a few appear to be subgiants. --- Paul Kuin NASA/ADC 1997 Feb 24 UNKNOWN UNKNOWN The data were received by the ADC in June 1996. The file names were changed to conform to the standards used. J_ApJS_105_419.xml Observations of double stars and new pairs. XVII. J/ApJS/105/475 J/ApJS/105/475 Observations of double stars. XVII. Observations of double stars and new pairs. XVII. W D Heintz Astrophys. J. Suppl. Ser. 105 475 1996 1996ApJS..105..475H J/ApJS/74/275 : Observations of double stars XIV (Heintz 1990) J/ApJS/83/351 : Observations of double stars. XV. (Heintz, 1992) Stars, double and multiple astrometry binaries: visual Micrometer observations of 722 doubles, including 14 new pairs, in 1994-1995 are tabulated, along with some orbits.
Orbits RAh Right ascension (2000.0) h RAdm Right ascension (2000.0) (deci-minutes) 0.1min DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin ADS ADS number --- Name Name of binary --- mag1 Visual magnitude of the primary mag mag2 Visual magnitude of the secondary mag SpType Spectral type --- Per Period yr T Time of perihelion passage yr a Semi-major axis arcsec e Eccentricity --- i Inclination angle deg omega Longitude of perihelion deg OMEGA Longitude of ascending node deg plx Dynamical parallax arcsec Micrometer Observations Name Star name --- RAh Right ascension (2000.0) h RAdm Right ascension (2000.0) (deci-minutes) 0.1min DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin ObsDate Date of observation yr PA Position angle deg Sep Separation between the components arcsec Nobs Number of nights --- m_Name Components for multiple systems --- m1 Magnitude of brightest component mag m2 Magnitude of second brightest component mag com Comments --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Jun 17 UNKNOWN UNKNOWN Prepared via OCR at CDS. Some magnitudes corrected in table2 on 19-Feb-1998 J_ApJS_105_475.xml An Atlas of H II Regions in Nearby Seyfert Galaxies J/ApJS/105/93 J/ApJS/105/93 H II Regions in Nearby Seyfert Galaxies An Atlas of H II Regions in Nearby Seyfert Galaxies I N Evans A P Koratkar T Storchi-Bergmann H Kirkpatrick T M Heckman A S Wilson Astrophys. J. Suppl. Ser. 105 93 1996 1996ApJS..105...93E Galaxies, Seyfert H II regions atlases galaxies: Seyfert HII regions Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.
Inventory H II regions NGC NGC number --- Num H II region number --- RAh Right ascension (J2000) number=1 Equatorial coordinates (equinox J2000) of the H II region image center of gravity in the Hubble Space Telescope Guide Star Catalog reference frame. h RAm Right ascension (J2000) number=1 Equatorial coordinates (equinox J2000) of the H II region image center of gravity in the Hubble Space Telescope Guide Star Catalog reference frame. min RAs Right ascension (J2000) number=1 Equatorial coordinates (equinox J2000) of the H II region image center of gravity in the Hubble Space Telescope Guide Star Catalog reference frame. s DE- Declination sign --- DEd Declination (J2000) number=1 Equatorial coordinates (equinox J2000) of the H II region image center of gravity in the Hubble Space Telescope Guide Star Catalog reference frame. deg DEm Declination (J2000) number=1 Equatorial coordinates (equinox J2000) of the H II region image center of gravity in the Hubble Space Telescope Guide Star Catalog reference frame. arcmin DEs Declination (J2000) number=1 Equatorial coordinates (equinox J2000) of the H II region image center of gravity in the Hubble Space Telescope Guide Star Catalog reference frame. arcsec Area Area of the H II region image number=2 These data values are for the H II region image above the lowest COSMOS threshold. arcsec2 Total Integrated pixel intensity (in digital number) number=2 These data values are for the H II region image above the lowest COSMOS threshold. --- Peak Peak pixel intensity (in digital number) number=2 These data values are for the H II region image above the lowest COSMOS threshold. --- e Ellipticity of the H II region image number=2 These data values are for the H II region image above the lowest COSMOS threshold. --- PA Position angle of the H II region image number=2 These data values are for the H II region image above the lowest COSMOS threshold. deg CDS 1997 Feb 10 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 16-Jul-96 J_ApJS_105_93.xml Rotation curves and velocity measures for spiral galaxies in pairs J/ApJS/106/27 J/ApJS/106/27 Spiral galaxies in pairs Rotation curves and velocity measures for spiral galaxies in pairs W C Keel Astrophys. J. Suppl. Ser. 106 27 1996 1996ApJS..106...27K VII/77 : Catalog of Pairs of Galaxies (CPG) (Karachentsev+ 1972) Galaxies, rotation galaxies: distances and redshifts galaxies: kinematics and dynamics galaxies: Seyfert galaxies: spiral Rotation curves have been obtained for 76 spiral galaxies in pairs, including a geometrically selected subset from the Karachentsev catalog and a set of Seyfert galaxies with close companions. Derived parameters of the rotation curves and the galaxies' light distributions are also presented. The rotation curves are classified broadly by shape, with special emphasis on kinematic disturbances and regions of solid-body behavior that may lead to bar development. Broadband images of the galaxies allow assessments of their degree of symmetry or disturbance. These velocity slices afford an empirical basis for evaluating the accuracy of radial velocity measures for spiral galaxies in pairs, and the dynamically important radial velocity differences. Specifically, the disagreement among several plausible ways of estimating the central velocity from these rotation data is used to estimate how closely any of these might approximate the nuclear or center-of-mass values. From seven indicators of central velocity, the internal scatter is delta_vv = 34 km/s. Of these, the velocity weighted by Halpha intensity along the slit shows a systematic offset of about 20 km/s with respect to the others for the Karachentsev pairs, in the sense that this measure is redshifted with respect to the other indicators. This is in the sense (but not of the total magnitude) required to account for statistical asymmetries in pair velocity differences. Individual scatter between the velocity indicators taken pairwise ranges from delta = 20 to 52 km/s. These results imply that emission-line data such as these cannot specify the center of mass or nuclear redshift at a level more accurate than this, even for arbitrarily precise velocity measurements, because it is not clear how the observed quantities relate to the desired measurement in a physical sense. No useful predictor of which galaxies have large or small scatter among velocity measures was found, except that the scatter is small for the class of "nonrotating" galaxies with small overall velocity amplitudes. Projected separation, separation normalized to disk scale length, and morphological disturbance do not correlate with velocity scatter.
Galaxy pair parameters CPG CPG (Cat. <VII/77>) name --- Name Other name --- n_CPG absorption --- PA Position angle deg HVcorr Correction to heliocentric velocity km/s Peak Adopted location along the slit from the continuum peak --- Velocity curves for galaxy pairs CPG CPG (Cat. <VII/77>) name --- Pixel Pixel number along the slit Pixel number along the slit, at a scale of 0.78 arcsecond/pixel. The slices are along the position angles indicated in the header records. Smaller pixel numbers are at the eastern end of the slit (that is, NNE for PA 10 degrees, SSE at PA 170). pix Vobs Weighted mean velocity in the relativistic convention km/s e_Vobs 2-sigma error derived from photon statistics km/s Halpha Total Halpha intensity Total H-alpha intensity in instrumental units (neglecting the broad-line component where it can be distinguished). --- Cont Continuum intensity --- Lines Number of emission lines measured --- Patricia Bauer CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 09-Oct-96 J_ApJS_106_27.xml A multiwavelength catalog of Seyfert 2 galaxies observed in the 2-10 keV energy band J/ApJS/106/399 J/ApJS/106/399 Seyfert 2 galaxies multiwavelength catalog A multiwavelength catalog of Seyfert 2 galaxies observed in the 2-10 keV energy band M Polletta L Bassani G MalagutI G G C Palumbo E Caroli Astrophys. J. Suppl. Ser. 106 399 1996 1996ApJS..106..399P VII/173 : Catalogue of Seyfert Galaxies (Lipovetsky+, 1988) Galaxies, Seyfert Galaxy catalogs X-ray sources catalogs galaxies: Seyfert X-rays: galaxies This paper is a catalog of Seyfert 2 galaxies observed in the 2-10keV band (339 flux entries). In total, it contains data on 150 objects; for 76 objects, a positive detection is reported, while for the remaining sources, 2{sigma} upper limits to the X-ray emission are given. Most of the data have been collected from the literature over a period starting from 1974 up to the middle of 1995. Accurate searches of literature and databases were performed for all objects, and frequently spectral fits were reevaluated in order to make the data in the catalog uniform and complete. Some unpublished data are also included. For six objects, EXOSAT/ME data have been extracted from the satellite database and analyzed; the 13 fluxes obtained have been added to the present catalog. The compilation of hard X-ray data has been complemented with data in the soft (0.1-3keV) X-ray band, as well as in ultraviolet (1450A), optical (5500A), infrared (3.5, 12, 25, 60, 100mm), and radio (6cm) bands. Fluxes of the [O III] {lambda}5007 and H{beta} emission lines as well as the Balmer decrement H{alpha}/H{beta}, and axial ratio a/b are also given. The present database is meant to be a useful tool for the study of the Seyfert 2 phenomenon in its various aspects.
Seyfert 2 galaxies in the catalog Seq Sequential number --- Name Galaxy name (NED) --- RA1950h Right ascension (1950) h RA1950m Right ascension (1950) min RA1950s Right ascension (1950) s DE1950- Declination sign --- DE1950d Declination (1950) deg DE1950m Declination (1950) arcmin DE1950s Declination (1950) arcsec RA2000h Right ascension (2000) h RA2000m Right ascension (2000) min RA2000s Right ascension (2000) s DE2000- Declination sign --- DE2000d Declination (2000) deg DE2000m Declination (2000) arcmin DE2000s Declination (2000) arcsec z Redshift --- n_z Note on z number=1 a: Awaki, 1991PASJ...43L..37A b: Kirhakos & Steiner, 1990AJ.....99.1435K c: Rego et al., 1993AJ....105..427R d: Kirhakos & Steiner, 1990AJ.....99.1722K e: Lipovetsky et al., 1987, Cat. <VII/173> f: SIMBAD database. g: Dahari & De Robertis, 1988ApJS...67..249D h: De Grijp et al., 1992A&AS...96..389D i: Chatzichristou & Vanderriest, 1995A&A...298..343C l: Mazzarella & Boroson, 1993ApJS...85...27M m: Mushotzky, 1982ApJ...256...92M n: Warwick et al., 1993MNRAS.265..412W --- Type Type --- TypeN NELG type --- n_Type Type source number=1 a: Awaki, 1991PASJ...43L..37A b: Kirhakos & Steiner, 1990AJ.....99.1435K c: Rego et al., 1993AJ....105..427R d: Kirhakos & Steiner, 1990AJ.....99.1722K e: Lipovetsky et al., 1987, Cat. <VII/173> f: SIMBAD database. g: Dahari & De Robertis, 1988ApJS...67..249D h: De Grijp et al., 1992A&AS...96..389D i: Chatzichristou & Vanderriest, 1995A&A...298..343C l: Mazzarella & Boroson, 1993ApJS...85...27M m: Mushotzky, 1982ApJ...256...92M n: Warwick et al., 1993MNRAS.265..412W --- b/a b/a axis ratio --- n_b/a Source of b/a number=1 a: Awaki, 1991PASJ...43L..37A b: Kirhakos & Steiner, 1990AJ.....99.1435K c: Rego et al., 1993AJ....105..427R d: Kirhakos & Steiner, 1990AJ.....99.1722K e: Lipovetsky et al., 1987, Cat. <VII/173> f: SIMBAD database. g: Dahari & De Robertis, 1988ApJS...67..249D h: De Grijp et al., 1992A&AS...96..389D i: Chatzichristou & Vanderriest, 1995A&A...298..343C l: Mazzarella & Boroson, 1993ApJS...85...27M m: Mushotzky, 1982ApJ...256...92M n: Warwick et al., 1993MNRAS.265..412W --- X-ray data in the 2-10 keV and 0.1-3 keV bands Seq Sequential number --- Name Object name --- InstA 2-10keV observations instrument --- n_InstA Note on InstA number=1 e: Possible contamination by cluster. l: Possible contamination by nearby source. --- Date2-10 Observation date for 2-10keV data "DD/MM/YY" n_Dateend If '-', interval of observation --- Dateend Last day of observation (when interval) --- n_Date2-10 Note on observation date number=2 a: EINLOG database (HEASARC). c: Average of more than one observation performed on the same date. d: Scan performed during the dates indicated. f: IPCLOG database (ESIS). g: ROSATPUBLIC database (ESIS). i: Average of more than one observation performed between the indicated dates. m: Fabbiano et al., 1992ApJS...80..531F Uhuru Survey period: 12/12/70-13/03/73; Ariel 5 survey period: 15/10/74-14/03/80; HEAO I survey period: 15/08/77-15/02/78 Einstein survey period: 13/11/78-/ /04/81 ROSAT survey period: 01/08/90-01/02/91 --- Obs2-10 S: Survey --- l_F2-10 Limit flag on F2-10 --- F2-10 Observed flux in the 2-10keV band 10-14W/m2 l_L2-10 Limit flag on L2-10 --- L2-10 Luminosity in the 2-10keV band 10+35W r_F2-10 Reference for 2-10keV data --- n_F2-10 Note on F2-10 number=3 b: Measurement uncertain due to the nonuniform exposure. It is probably underestimated. h: Flux computed using the spectral parameters reported in Halpern, 1982, Ph.D. thesis, Harward Univ. A: For 25 NGC 1275, F0.1-3 = 21/52 10-14W/m2; L0.1-3 = 281/697 10+35W --- InstB 0.1-3keV observations instrument --- n_InstB Note on InstB number=1 e: Possible contamination by cluster. l: Possible contamination by nearby source. --- Date0.1-3 Observation date for 0.1-3keV data "DD/MM/YY" n_Date2 If '-', interval of observation --- Date2 Date of the end of observation "DD/MM/YY" n_Date0.1-3 Note on observation date --- Obs0.1-3 S: Survey; W: SLEW --- l_F0.1-3 Limit flag on F0.1-3 --- F0.1-3 Observed flux in the 0.1-3keV band 10-14W/m2 n_F0.1-3 Note on F0.1-3 number=3 b: Measurement uncertain due to the nonuniform exposure. It is probably underestimated. h: Flux computed using the spectral parameters reported in Halpern, 1982, Ph.D. thesis, Harward Univ. A: For 25 NGC 1275, F0.1-3 = 21/52 10-14W/m2; L0.1-3 = 281/697 10+35W --- l_L0.1-3 Limit flag on L0.1-3 --- L0.1-3 Luminosity in the 0.1-3keV band 10+35W n_L0.1-3 Note on L0.1-3 number=3 b: Measurement uncertain due to the nonuniform exposure. It is probably underestimated. h: Flux computed using the spectral parameters reported in Halpern, 1982, Ph.D. thesis, Harward Univ. A: For 25 NGC 1275, F0.1-3 = 21/52 10-14W/m2; L0.1-3 = 281/697 10+35W --- r_F0.1-3 Reference for 0.1-3keV data --- *Spectral indices assumed in equation Ref1 Reference number --- n_Ref1 Note on Ref1 number=1 b: Fluxes computed from count rates. --- Ref2 Reference number --- Ref3 Reference number --- n_Ref3 Note on Ref3 number=1 b: Fluxes computed from count rates. --- Ref4 Reference number --- SI Spectral index --- n_SI2 "/" if interval, "," if two values --- SI2 Upper value of SI interval or second value --- n_SI Note on Spectral index number=2 a: Spectral indices assumed for single object are reported in the reference. c: For the following sources the specified spectral index was assumed: for ESO 033-G002, NGC 1068, NGC 4945, Mrk 507, NGC 7314, values reported by Boller et al. (1992A&A...261...57B) for NGC 1614, NGC 1672, Mrk 78, Mrk 273, Mrk 463E, values reported by Kruper, Urry, & Canizares (1990ApJS...74..347K) for NGC 5033, NGC 5256, NGC 6240, average value (1.91) reported by Brinkmann et al. (1995A&AS..109..147B) d: 1.91 for NGC 5033 (Brinkman et al., 1995A&AS..109..147B) and 2.3 for NGC 5273 (Boller et al., 1992A&A...261...57B) --- Inst Instrument --- E1 Lower value of energy range keV --- Separation dash --- E2 Upper value of energy range keV Optical and radio observed fluxes Seq Sequential number --- Name Object name --- Vmag V magnitude (NED) mag n_Vmag Note on Vmag number=1 d: Veron-Cetty & Veron, 1986A&AS...66..335V --- l_Ha/Hb Limit flag on Ha/Hb --- Ha/Hb H{alpha}/H{beta} fluxes ratio --- n_Ha/Hb Note on Ha/Hb number=2 b: Osterbrock & Martel, 1993ApJ...414..552O e: Brindle et al., 1990MNRAS.244..577B f: Dahari & De Robertis, 1988ApJS...67..249D g: Elvis et al., 1978MNRAS.183..129E h: F(H{alpha}) from Dahari, 1985AJ.....90.1772D i: Phillips et al., 1983ApJ...266..485P l: De Grijp et al., 1992A&AS...96..389D n: Ward et al., 1988ApJ...324..767W o: Bartel et al., 1984ApJ...279..112B --- l_log(F[OIII]) Limit flag on log(F[OIII]) --- log(F[OIII]) [OIII] flux [mW/m2] n_log(F[OIII]) Note on log(F[OIII]) number=1 d: Veron-Cetty & Veron, 1986A&AS...66..335V --- l_log(FHb) Limit flag on log(FHb) --- log(FHb) H{beta} flux [mW/m2] r_log(FHb) References for log(FHb) and log(F[OIII]) --- l_log(F6cm) Limit flag on log(F6cm) --- log(F6cm) 6cm flux [mJy] n_log(F6cm) Note on log(F6cm) number=3 c: 4.75 GHz m: 4.85 GHz --- r_log(F6cm) Reference for log(F6cm) --- IR and UV data Seq Sequential number --- Name Object name --- l_F12um Limit flag on F12um --- F12um 12{mu}m flux Jy n_F12um Note on F12um number=1 g: Gezari et al., 1993, See Cat. <II/209> --- l_F25um Limit flag on F25um --- F25um 25{mu}m flux Jy l_F60um Limit flag on F60um --- F60um 60{mu}m flux Jy l_F100um Limit flag on F100um --- F100um 100{mu}m flux Jy n_F100um Note on F100um number=2 f: Kirhakos & Steiner, 1990AJ.....99.1722K h: Lonsdale et al., 1985R, Catalogued Galaxies and Quasars observed in the IRAS survey. i: Lawrence & Elvis, 1982ApJ...256..410L --- r_F12um Reference for 12 to 100 {mu}m fluxes --- l_F3.5um Limit flag on F3.5um --- F3.5um 3.5 {mu}m flux 10-2Jy n_F3.5um Note on F3.5um number=3 a: 3.69 mm b: 3.4 mm d: 3.8 mm e: 3.7 mm l: 3.82 mm --- r_F3.5um Reference for 3.5{mu}m flux --- n_r_F3.5um *: Density flux computed from magnitude (see text) --- l_F1450A Limit flag on F1450A --- F1450A 1450A flux (or 1455A if n_F1450A = c) 10-4Jy n_F1450A c: flux at 1455 A --- r_F1450A Reference for 1450A flux --- References to tables 1-5 by reference number No Reference number --- BibCode BibCode --- Aut Author's names --- Com Comments --- James Marcout, Patricia Bauer CDS 1997 Sep 05 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_106_399.xml SiO maser sources in the outer disk of the Galaxy J/ApJS/106/463 J/ApJS/106/463 SiO maser sources SiO maser sources in the outer disk of the Galaxy B W Jiang S Deguchi I Yamamura Y Nakada S H Cho T Yamagata Astrophys. J. Suppl. Ser. 106 463 1996 1996ApJS..106..463J Infrared sources Masers Photometry, infrared Galaxy: kinematics and dynamics ISM: molecules masers stars: spectral classification stars: variables: other (long-period variables) The observations in the 28SiO J=1-0 v=1, J=1-0 v=2 lines and the 29SiO J=1-0, v=0 lines were simultaneously made toward 181 color-selected IRAS sources in the outer disk of the Galaxy (at longitudes between 90 deg and 250 deg). The 28SiO lines were detected in 63 sources (56 new) and the 29SiO line in 11 sources (9 new). Most of the detections are optically variable stars, mainly Mira-type variables and a few semiregular variables. The detection rate (35%) is much lower than that of the bulge survey performed by the same observational system - the 45m telescope at Nobeyama Radio Observatory. The lower detection rate of SiO maser emission is partly attributed to the increase of contaminations by stars with C-rich circumstellar envelopes and young stellar objects in the outer disk sample. The kinematical implications of the observational results are also discussed. The luminosity distances to the SiO maser sources are estimated from their IRAS fluxes at 12um and colors. By combining the SiO radial velocity and the luminosity distance, the rotation curve of the outer Galactic disk is found to be slightly falling within the Galactocentric distance between 8.5 and 12kpc. The sources located within 20deg from the Galactic anticenter direction are used to check for a peculiar motion of the local standard of rest.
Line parameters of Gaussian components of the v=1 and v=2 detections Line parameters of Gaussian components of the 29SiO detections IRAS IRAS PSC (Cat. <II/125>) name --- TA1 Peak antenna temperature number=1 Gaussian components for SiO v = 1 J = 1-0 line. K n_TA1 : when no data for TA1 --- rms1 1 sigma noise level of line observation number=1 Gaussian components for SiO v = 1 J = 1-0 line. K Vlsr1 Velocity in Local Standard of Rest number=1 Gaussian components for SiO v = 1 J = 1-0 line. km/s n_Vlsr1 : when no data for Vlsr1 --- FWHM1 Full width at half maximum number=1 Gaussian components for SiO v = 1 J = 1-0 line. km/s n_FWHM1 : when no data for FWHM1 --- TA2 Peak antenna temperature number=2 Gaussian components for SiO v = 2 J = 1-0 line. K n_TA2 : when no data for TA2 --- rms2 1 sigma noise level of line observation number=2 Gaussian components for SiO v = 2 J = 1-0 line. K Vlsr2 Velocity in Local Standard of Rest number=2 Gaussian components for SiO v = 2 J = 1-0 line. km/s n_Vlsr2 : when no data for Vlsr2 --- FWHM2 Full width at half maximum number=2 Gaussian components for SiO v = 2 J = 1-0 line. km/s n_FWHM2 : when no data for FWHM2 --- Infrared properties and observation parameters of the nondetections IRAS IRAS PSC (Cat. <II/125>) name number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> --- GLon Galactic longitude number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> deg GLat Galactic latitude number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> deg F12 IRAS flux at 12 microns number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> Jy C12 IRAS color C12 (log F25/F12) number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> --- C23 IRAS color C23 (log F60/F25) number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> --- Var IRAS variability index number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> --- LRS IRAS Low Resolution Spectrum class number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> --- Id ID status; 1=identified; 0=unidentified number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> --- rms1 1-sigma level for SiO maser v=1 line obs. number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> K rms2 1-sigma level for SiO maser v=2 line obs. number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> K Date Date of SiO maser observation, yymmddhh number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> --- Other Result of obs. in other molecular lines Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> number= Results of observations in other molecular lines, '+' means positive result and '-' means negative, number in parentheses are reference numbers, as follows: 1. te Lintel Hekkert et al., 1991A&AS...90..327T 2. Le Sequeren et al., 1992A&A...254..133L 3. Eder et al., 1988ApJS...66..183E 4. Lewis et al., 1990ApJ...362..634L 5. Chengalur et al., 1993ApJS...89..189C 6. Lewis, 1994ApJS...93..549L 7. Loup et al., 1993A&AS...99..291L 8. Wouterlout et al., 1989A&AS...80..149W, Cat. <J/A+AS/80/149> 9. Sivagnanam et al., 1990A&A...233..112S 10. Galt et al., 1989AJ.....98.2182G 11. Nyman et al., 1993A&A...280..551N 12. Benson et al., 1990ApJS...74..911B, Cat. <V/68> 13. Kastner et al., 1993A&A...275..163K, Cat. <J/A+A/275/163> --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 09-Nov-96 J_ApJS_106_463.xml The Molonglo Reference Catalog/1 Jansky radio source survey. I. Radio galaxy identifications. J/ApJS/107/19 J/ApJS/107/19 MRC/1Jy Radio source survey. I. The Molonglo Reference Catalog/1 Jansky radio source survey. I. Radio galaxy identifications. P J McCarthy V K Kapahi W Van Breugel S E Persson R Athreya C R Subrahmanya Astrophys. J. Suppl. Ser. 107 19 1996 1996ApJS..107...19M VIII/16 : Molonglo Reference Catalogue of Radio Sources (Large+ 1991) Galaxies, radio Magnitudes Redshifts galaxies: photometry quasars: general radio continuum: galaxies surveys This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408>0.95Jy and -30<decl.(1950)<-20, and 9h20m<R.A.(1950)<14h4m or 20h20m<R.A.(1950)<6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.
Optical positions of MRC/1 Jy radio galaxies MRC Designation as in MRC <VIII/16> number=1 For sources noted as "Unidentified" we list the radio position as derived from either our VLA images or from the MRC when observations are not available. Positions listed to the nearest arcsecond of declination are all radio positions are are flagged 'R' in byte 34. The n_MRC suffix were assigned lower-case letters (a, b, c) in byte 10 for those MRC names which had no suffix in the original MRC. --- m_MRC Radio Multiplicity as in MRC number=1 For sources noted as "Unidentified" we list the radio position as derived from either our VLA images or from the MRC when observations are not available. Positions listed to the nearest arcsecond of declination are all radio positions are are flagged 'R' in byte 34. The n_MRC suffix were assigned lower-case letters (a, b, c) in byte 10 for those MRC names which had no suffix in the original MRC. --- n_MRC Optical Multiplicity number=1 For sources noted as "Unidentified" we list the radio position as derived from either our VLA images or from the MRC when observations are not available. Positions listed to the nearest arcsecond of declination are all radio positions are are flagged 'R' in byte 34. The n_MRC suffix were assigned lower-case letters (a, b, c) in byte 10 for those MRC names which had no suffix in the original MRC. --- RAh Right ascension (1950) number=1 For sources noted as "Unidentified" we list the radio position as derived from either our VLA images or from the MRC when observations are not available. Positions listed to the nearest arcsecond of declination are all radio positions are are flagged 'R' in byte 34. The n_MRC suffix were assigned lower-case letters (a, b, c) in byte 10 for those MRC names which had no suffix in the original MRC. h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) number=1 For sources noted as "Unidentified" we list the radio position as derived from either our VLA images or from the MRC when observations are not available. Positions listed to the nearest arcsecond of declination are all radio positions are are flagged 'R' in byte 34. The n_MRC suffix were assigned lower-case letters (a, b, c) in byte 10 for those MRC names which had no suffix in the original MRC. deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec RadioPos 'R' indicates a radio position number=1 For sources noted as "Unidentified" we list the radio position as derived from either our VLA images or from the MRC when observations are not available. Positions listed to the nearest arcsecond of declination are all radio positions are are flagged 'R' in byte 34. The n_MRC suffix were assigned lower-case letters (a, b, c) in byte 10 for those MRC names which had no suffix in the original MRC. --- z Redshift --- u_z Uncertainty flag on z --- l_rmag Limit flag on rmag --- rmag r magnitude number=2 All of the magnitudes listed are measured in a 4" diameter aperture in the Thuan-Gunn r- band, even when the image shown in Fig.1 is in a different pass-band. mag u_rmag Uncertainty flag on rmag --- Filt Filter --- FOV Field of view codes number=4 Field of view (FOV) codes are as follow: 1 = 66"x66"(2.5m+TI), 2 = 87"x 87"(m+TI), 3 = 71"x71"(2.5m+IR), 4 = 170"x 170"(Sky Survey), 5 = 59"x 59"(2.5m+Tek No.1), 6 = 51"x 51"(2.5m+Tek No.2),7 = other. --- Run Run numbers number=3 The run numbers denoted by asterisks are IR imaging runs that will be described elsewhere. --- Note Note detailed in file notes.dat --- Rem Remark --- Notes of table2 MRC MRC designation as in file table2.dat --- m_MRC Multiplicity index on MRC --- Text Text of the note --- James Marcout, Patricia Bauer CDS 1998 Jan 28 We thank H. Andernach <heinz@astro.ugto.mx> for proofreading the table, and supplying the remarks in columns m_MRC and RadioPos UNKNOWN UNKNOWN Prepared via OCR at CDS (August 1997) J_ApJS_107_19.xml The morphologies of distant galaxies. II. Classifications from the Hubble space telescope medium deep survey. J/ApJS/107/1 J/ApJS/107/1 Morphologies of distant galaxies II The morphologies of distant galaxies. II. Classifications from the Hubble space telescope medium deep survey. R G Abraham S Van den Bergh K Glazebrook R S Ellis B X Santiago P Surma R E Griffiths Astrophys. J. Suppl. Ser. 107 1 1996 1996ApJS..107....1A Galaxies, photometry Morphology galaxies: evolution galaxies: fundamental parameters galaxies: interactions surveys The morphological properties of high-redshift galaxies are investigated using a sample of 507 objects (I<22.0mag) from the Hubble Space Telescope (HST) Medium Deep Survey. Independent visual morphological classifications for each galaxy are used to quantify the statistical uncertainties in the galaxy classifications. Visual classifications are found to agree well for I<21mag. Fainter than I=21mag significant disagreements are seen in the independent visual classifications of late-type systems with T>7, merging systems, and peculiar galaxies. The classifications of these systems are shown to be somewhat subjective. Objective classifications based upon measurements of central concentration and asymmetry for the Medium Deep Survey sample are presented. These classifications are calibrated using measurements of structural parameters for an artificially redshifted sample of local objects. Morphologically segregated number counts using both sets of visual classifications and objective classifications support the conclusion that the observed galaxy counts agree with no-evolution predictions for the elliptical and spiral populations, as reported in Glazebrook et al. (1995MNRAS.275L..19G). A major conclusion is that the large overdensity of merging/peculiar/irregular galaxies relative to the predictions of no-evolution models (reported by Glazebrook et al. 1995MNRAS.275L..19G) is confirmed. However, the shape of the faint-end (I>21.0mag) number count relation for peculiar objects is sensitive to the large systematic uncertainties inherent in the visual classification of these objects. Despite this caveat, the frequency of objects showing clear evidence for tidal interactions (e.g., tidal tails) in the HST sample is at least 50% larger than it is among nearby galaxies, at the 2{sigma} level. Relatively few "chain galaxies" are seen among the sample of peculiar objects, suggesting that these systems do not form a large component of the peculiar galaxy population at I<22mag.
HST
Catalog of morphological classifications ID Identification --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Imag I magnitude mag C Central concentration --- A Rotational asymmetry --- RSE Ellis (1990, ASP Conf. vol 10, 248) classification number=1 -2: star -1: compact 0: E 1: E/S0 2: S0 3: Sab 4: S 5: Scdm 6: Ir 7: peculiar 8: merger 9: defect --- n_RSE Note number=2 uem0-38 : Image shows two nuclei and tidal tails. This is clearly an interacting/merging pair uem0-45 : No obvious signs of interaction. uy40-41 : Nucleus too large for Sc classification. uy40-53 : This is not a low surface brightness spiral. uy40-60 : No direct evidence for interactions. ux40-26 : Type Sc assigned because of small nucleus and faint disk. However, no spiral arms are visible ux40-106: Probably S0 rather than Sc because no arms are visible. ubi1-31 : No sign of tidal arms, so probably not a merger. ubi1-64 : Not an image defect. ueh0-10 : Not as compact as an elliptical. ucs0-1 : This appears to be a partly resolved Ir galaxy rather than a merger remnant. uop0-40 : It has a nucleus, so it must be a spiral. uui0-29 : This is an Sa spiral. uui0-38 : This may be a partly resolved Ir galaxy. uui0-51 : Edge-on dwarf irregular. Not an image deSect. uui0-75 : Merger remnant? Has two nuclei and one spiral arm. umd4-76 : Appears to be a low surface brightness dE3. --- VDB van den Bergh (1960ApJ...131..215V & 1960ApJ...131..558V) classification number=1 -2: star -1: compact 0: E 1: E/S0 2: S0 3: Sab 4: S 5: Scdm 6: Ir 7: peculiar 8: merger 9: defect --- Class Classification of van den Bergh (1960PDDO....2..159V) in DDO system --- Com VDB comment --- James Marcout, Patricia Bauer CDS 1997 Aug 28 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_107_1.xml The Stromlo-APM Redshift Survey IV: The Redshift Catalogue J/ApJS/107/201 J/ApJS/107/201 The Stromlo-APM Redshift Survey IV The Stromlo-APM Redshift Survey IV: The Redshift Catalogue J Loveday B A Peterson S J Maddox G Efstathiou Astrophys. J. Suppl. Ser. 107 201 1996 1996ApJS..107..201L Galaxy catalogs Photometry Redshifts The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J) < 17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3 sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V = 1.38 million Mpc^3/h^3.
Galaxies in Stromlo-APM survey ID Galaxy name number=1 Each galaxy name is composed of the survey field number and the x, y position of the galaxy on the plate---this should ease location of any particular galaxy on the plate material. The first 3 digits are the SERC field number. The second set of digits are the x-position in millimetres from the centre of the plate (actually the APM scan centre). These are preceded by a `+' sign for galaxies to the right (west) of the plate centre or by a `-' sign for galaxies to the left (east) of centre. The final 3 digits are the y position, again in mm from the plate centre. A preceding `-' indicates galaxies above (north) of the plate centre, `+' indicates galaxies below (south) of the centre. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (arcminutes) arcmin DEs Declination 1950 (arcseconds) arcsec Bj Bj magnitude mag D-MAJ Major diameter arcsec D-MIN Minor diameter arcsec PA Position angle (degrees) number=2 PA is measured clockwise from south-north line. deg MType Morphological type number=3 The morphological type is given by mod(Mtype,10) 1 = Elliptical 2 = Lenticular 3 = Spiral 4 = Irr/Pec 5 = Uncertain 8 = Merged with star 9 = Multile galaxy Galaxies from the ESO catalogue have 10 added, those assigned morphological types by SJM have 20 added (all others typed by JL). --- RV Radial velocity (heliocentric) km/s e_RV Error in radial velocity km/s r_RV Source of radial velocity number=4 The RV_src flag indicates the source of the radial velocity: -1 = unreliable 0 = not available 1 = MSSSO 2.3m, absorption features 2 = MSSSO 2.3m, emission lines 3 = MSSSO 2.3m, both absorption and emission 4 = Southern Sky Redshift Survey 5 = Dressler & Schectman 1988 6 = Huchra's ZCAT compilation --- Field centres Field SERC field number number= This table lists SERC field centres in 1950 decimal degrees. The column labeled RAextent gives the half-size of the Right Ascension of the field in degrees. The DEextent is 2.5 degrees for every field. This list of fields may be used for example to generate a random catalogue with the same boundaries as the survey data as follows. A point with coordinates (RAp, DEp) is inside a field with coordinates (RAf, DEf) if (abs(RAp - RAf) < RAextent) and (abs(DEp - DEf) < DEextent). An additional test should be made to allow for the extra overlap between fields at RA = 0. If RAf is not zero then abs(RAp) must be greater than RAextent. --- RAdeg RA of field centre 1950 (degrees) number= This table lists SERC field centres in 1950 decimal degrees. The column labeled RAextent gives the half-size of the Right Ascension of the field in degrees. The DEextent is 2.5 degrees for every field. This list of fields may be used for example to generate a random catalogue with the same boundaries as the survey data as follows. A point with coordinates (RAp, DEp) is inside a field with coordinates (RAf, DEf) if (abs(RAp - RAf) < RAextent) and (abs(DEp - DEf) < DEextent). An additional test should be made to allow for the extra overlap between fields at RA = 0. If RAf is not zero then abs(RAp) must be greater than RAextent. deg DEdeg Dec of field centre 1950 (degrees) number= This table lists SERC field centres in 1950 decimal degrees. The column labeled RAextent gives the half-size of the Right Ascension of the field in degrees. The DEextent is 2.5 degrees for every field. This list of fields may be used for example to generate a random catalogue with the same boundaries as the survey data as follows. A point with coordinates (RAp, DEp) is inside a field with coordinates (RAf, DEf) if (abs(RAp - RAf) < RAextent) and (abs(DEp - DEf) < DEextent). An additional test should be made to allow for the extra overlap between fields at RA = 0. If RAf is not zero then abs(RAp) must be greater than RAextent. deg RAextent RA extent of field (degrees) number= This table lists SERC field centres in 1950 decimal degrees. The column labeled RAextent gives the half-size of the Right Ascension of the field in degrees. The DEextent is 2.5 degrees for every field. This list of fields may be used for example to generate a random catalogue with the same boundaries as the survey data as follows. A point with coordinates (RAp, DEp) is inside a field with coordinates (RAf, DEf) if (abs(RAp - RAf) < RAextent) and (abs(DEp - DEf) < DEextent). An additional test should be made to allow for the extra overlap between fields at RA = 0. If RAf is not zero then abs(RAp) must be greater than RAextent. deg Holes drilled around big bright objects Field SERC field number number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif --- HOLX1 RA of 1st corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLY1 Dec of 1st corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLX2 RA of 2nd corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLY2 Dec of 2nd corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLX3 RA of 3rd corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLY3 Dec of 3rd corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg Jon Loveday Fermilab 1996 Apr 24 J_ApJS_107_201.xml An Atlas of Hubble Space Telescope Ultraviolet Images of Nearby Galaxies J/ApJS/107/215 J/ApJS/107/215 UV Images of Nearby Galaxies An Atlas of Hubble Space Telescope Ultraviolet Images of Nearby Galaxies D Maoz A V Filippenko L C Ho D Macchetto H Rix D P Schneider Astophys. J. Suppl. 107 215 1996 1996ApJS..107..215M Galaxies, nearby The accompanying tables are part of a pictorial atlas of UV (2300A) images, obtained with the Hubble Space Telescope (HST) Faint Object Camera, of the central 22"X22" of 110 galaxies. The observed galaxies are an unbiased selection constituting about one half of a complete sample of all large (D>6') and nearby (V< 2000 km/s) galaxies. This is the first extensive UV imaging survey of normal galaxies. The data are useful for studying star formation, low-level nuclear activity, and UV emission by evolved stellar populations in galaxies. At the HST resolution (0.05"), the images display an assortment of morphologies and UV brightnesses. These include bright nuclear point sources, compact young star clusters scattered in the field or arranged in circumnuclear rings, centrally-peaked diffuse light distributions, and galaxies with weak or undetected UV emission. We measure the integrated 2300A flux in each image, and classify the UV morphology. The UV and optical parameters are given in the tables.
HST
The atlas NGC NGC number --- arch a indicates an archival image An "a" denotes archival images, generally obtained with a different FOC format, filter, or exposure time than those of the program galaxies. --- UGC UGC number (northern galaxies only) --- ra_id 1950 right ascension for identification 1950 coordinates, to one-minute accuracy, as listed in the UGC and ESO catalogs. This datum can be useful for unambiguously identifying the galaxies in these and other catalogs, since listed coordinates for such large galaxies may vary by arcminutes from catalog to catalog. Also, some galaxies in the ESO catalog are designated solely by means of these coordinates. --- dec_id 1950 declination for identification --- RAh Right ascension hours (J2000) h RAm Right ascension minutes (J2000) min RAs Right ascension seconds (J2000) Coordinates of the nucleus, as measured in the STScI GASP system. These coordinates are generally accurate to 1"-2". s DE- Declination sign (J2000) --- DEd Declination degrees (J2000) deg DEm Declination minutes (J2000) arcmin DEs Declination seconds (J2000) arcsec vel_h Heliocentric velocity Heliocentric velocity, as listed in the UGC or ESO catalogs, in km/s. The selection criterion for inclusion in the sample was vel_h < 2000 km/s. km/s Dmaj Major axis diameter from UGC and ESO In tenths of arcminutes, from the UGC and ESO catalogs. The selection criterion for inclusion in the sample was Dmaj > 60. darcmin Dmin Minor axis diameter from UGC and ESO darcmin B B magnitude from UGC and ESO mag T Hubble type Hubble type, using de Vaucouleurs' T-type classification from the RC3 catalog (de Vaucouleurs et al. 1991). The correspondence is approximately as follows: E = -6 to -4 S0 = -3 to 0 Sa = 1 Sb = 3 Sc = 5 Sd = 7 Irr = 10 --- class Hubble type Hubble type and luminosity class using the classification, when available, from the Revised Shapley-Ames Catalog of Bright Galaxies (Sandage & Tammann 1987). --- lum Luminosity class For northern galaxies only, the bytes 81-82 contain the spectral classification of the nucleus, from Ho et al. (1995, 1996a). The designation is as follows. L = LINER (low-ionization nuclear emission-line region) H = H II nucleus T = "transition" source, between LINER and HII S = Seyfert nucleus A = "absorption-line" nucleus with no detected emission lines. : = an uncertain classification. The Ho et al. classification is based on the Filippenko & Sargent (1985, 1986) optical spectroscopic survey of the nuclei of a flux-limited (B < 12.5 mag) sample of 486 northern galaxies. All but three of the northern galaxies in the HST survey (which is diameter- and redshift-limited) are included in the Filippenko & Sargent (1985) sample. The effective aperture of the optical observations is 2"X4". The Ho et al. (1996a) classification is assigned after careful subtraction of absorption-line template spectra, leaving behind only the emission-line residual; see Ho et al. (1996a) for further details. --- date HST UT observation date --- root Image rootname in HST archive --- flux Total flux at 2270A Total f(lambda(2270A)) in units of 10^-15 erg/s/cm-2/A integrated above the background over the entire area of the image, and 1sigma uncertainty. The area of each image is 22"X 22", except for some of the archival exposures. The background was determined as follows. The mean counts per pixel were measured in seventeen 200X200-pixel squares in the frame, excluding occulting fingers and distortions in the FOC field (see Baxter et al. 1994), and the median counts per pixel were measured over the entire exposed part of the frame. The mean of the two lowest among these 18 measurements was used as the background value, and the standard deviation of the five lowest among the 18 measurements was used as the uncertainty in the background. The uncertainty in the background was propagated to an uncertainty on the total net counts in the image. The count rate above the background was converted to a UV flux density as described in S 2. The flux uncertainty due to the background uncertainty was combined in quadrature with a 5% absolute calibration uncertainty (Meurer 1995) to produce the quoted flux uncertainty. Except for bright and concentrated sources, the flux uncertainty is dominated by the uncertainty in the background determination. The cause of artificial background variations across the image is imperfect flat-fielding. Furthermore, a systematic error in background determination is unavoidable due to the small field of view, which covers only a fraction of the optical extent of these galaxies. Some of this systematic error is accounted for by the above procedure for estimating the background uncertainty. Nevertheless, the total UV fluxes quoted here agree well with the 2300 AA fluxes measured for those galaxies that have also been observed with IUE (Kinney et al. 1993; see also Meurer 1995), which has a comparable entrance aperture. This suggests that the regions of the images with the lowest counts are, in fact, devoid of significant UV emission. The UV fluxes given here should be used with care, and in conjunction with the UV-morphology classification and the visual appearance of the image. For example, there is low significance to the flux that is listed for a galaxy whose image appears blank. The UV fluxes are uncorrected for Milky Way or external extinction. aW/m2/10-10m u_flux One sigma uncertainty on flux aW/m2/10-10m morph UV morphology from HST image UV morphology roughly describing the HST image, with the following symbols. B = blank image W = weak or nearly absent UV emission S = star-forming morphology, with knots and compact sources of UV emission F = diffuse, centrally concentrated emission P = unresolved nuclear point-source R = circumnuclear star-forming ring Some comments from the original authors on each of these types follow. We have rechecked the coordinates and pointing of the blank ("B" morphology) images, and verified that they are not cases of telescope mispointing. As a check on the pointing accuracy, there are about 40 images which display a feature that can be securely associated with the nucleus of the galaxy. In almost all cases it is within 3" of the center of the image, as expected from the combined uncertainty in the GASP coordinates of the nucleus and the HST pointing accuracy. In the few cases where the nucleus is further from the image center, this has been traced to inaccurate input coordinates. The blank images are also not the result of foreground Milky-Way extinction, except for two galaxies, NGC 1560 and NGC 6946, which lie near the Galactic plane. Dust in the disks of the galaxies themselves is probably a factor, since 10 out of 13 galaxies with B morphologies have minor-to-major axis ratios less than 0.5 (i.e., an inclination >60deg). The fact that the centers of many galaxies are weak UV emitters is confirmed by the detection of very weak ("W-type") but significant and centrally concentrated emission in many of the galaxies, which establishes that the galactic nucleus is, indeed, in the field of view. The compact sources seen in the "S-type" morphologies are probably compact young star clusters, or in some cases individual O and B stars. Similar objects have been detected with HST in a variety of starburst environments (e.g., Meurer et al. 1995; Maoz et al. 1996). They will be studied in further detail by Ho et al. (1996b). The diffuse "F-type" emission occurs in some of the early-type spirals and the ellipticals in the sample. We believe that, in general, this observed feature is dominated by actual UV emission from an evolved spheroidal stellar population (the "UV-upturn"; see, e.g., Burstein et al. 1988), rather than visual-band emission leaking through the F220W filter, based on several tests described in S 2. In individual cases, however, confirmation by means of blue and near-UV imaging photometry of the center of each of these galaxies is required. Galaxies with bright nuclear UV point sources ("P-type") have been discussed in detail by Maoz et al. (1995), especially in the context of low-luminosity AGNs. They showed that 20% of the northern LINER galaxies display a nuclear point source in the FOC images, with a UV flux that, if extrapolated beyond the Lyman limit, could be sufficient to produce the observed strength of optical emission lines through photoionization. While this was the first direct detection of what may be the AGN-like ionizing source in LINER galaxies, it raised the question of why such a source is not detected in 80% of LINERs. Several of the P-type sources in in this paper, especially the weak ones and those in archival images, were not included in Maoz et al. (1995). However, the fraction of "UV-bright" LINERs, or LINERs plus Seyferts, remains unchanged. For example, among the 35 northern galaxies with spectral classification T, L, or S (transition-type, LINER, or Seyfert), nine have a nuclear UV point source. The five circumnuclear rings in the sample (designated "R") have been discussed in detail by Maoz et al. (1996), who showed that a large, possibly dominant fraction of the UV light in these objects is emitted by the numerous compact sources distributed along the rings. These sources are probably young and massive star clusters that will remain bound, similar to those seen with HST in other starburst environments. --- N.G. Roman ADC/SSDOO 1997 Feb 24 J_ApJS_107_215.xml A Westerbork synthesis radio telescope 327 MHz survey of the galactic plane. J/ApJS/107/239 J/ApJS/107/239 327 MHz survey of the galactic plane A Westerbork synthesis radio telescope 327 MHz survey of the galactic plane. A R Taylor W M Goss P H Coleman F van Leeuwen B J Wallace Astrophys. J. Suppl. Ser. 107 239 1996 1996ApJS..107..239T http://www.ras.ucalgary.ca/wsrt_survey.html : Images and FITS files H II regions Radio sources HII regions planetary nebulae: general radio continuum: general surveys (from the authors) The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey a section of the galactic plane at a radio frequency of 327MHz. Twenty-three overlapping synthesis fields were observed, covering galactic co-ordinates 43{deg}<l<91{deg}, |b|<1.6{deg}. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaiced to produce a single image of the entire survey region. Sensitivity of the mosaic is typically a few mJy. Resolution is 1' by 1'cosec(dec). The survey image provides our first high resolution view of the Galaxy at low radio frequencies, and includes sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, HII regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes less than about 3'.
Catalogue of small diameter sources Source Name of source --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s e_RAs Mean error on RA s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec e_DEs Mean error on Declination arcsec S367 Flux density at 367MHz mJy e_S367 Mean error on S367 mJy MajDiam Diameter (major) arcsec MinDiam Diameter (minor) arcsec PA Position Angle deg GLON Galactic longitude deg GLAT Galactic latitude deg IRAS identification Name Name from IRAS position --- Sep Separation from radio position arcsec S327MHz Flux density at 327MHz mJy e_S327MHz rms uncertainty on S327MHz mJy S12um Flux density at 12{mu}m mJy S25um Flux density at 25{mu}m mJy S60um Flux density at 60{mu}m mJy S100um Flux density at 100{mu}m mJy log(S25um/S12um) S25um/S12um ratio --- log(S60um/S25um) S60um/S25um ratio --- R S60um/S327MHz ration --- SI Radio spectral index --- Francois Ochsenbein CDS 1997 Feb 25 UNKNOWN UNKNOWN wsrt.dat copied from http://www.ras.ucalgary.ca/wsrt/wsrt.cat in February 1997 table1 sending by Russ Taylor <russ@grizzly.ras.ucalgary.ca> J_ApJS_107_239.xml A spectral atlas of hot, luminous stars at 2 microns J/ApJS/107/281 J/ApJS/107/281 Atlas of hot, luminous stars at 2 microns A spectral atlas of hot, luminous stars at 2 microns M M Hanson P S Conti M J Rieke Astrophys. J. Suppl. Ser. 107 281 1996 1996ApJS..107..281H Spectra, infrared Stars, luminous atlases infrared: stars stars: early-type stars: fundamental parameters We present 2um (K band) spectra of 180 well-studied, optically visible, luminous stars. Most of the stars are of OB spectral type, but we have also included a number of Oe and Be stars, OBN and OBC stars, cool hypergiant stars, and high-mass X-ray binary stars. Our aim in studying normal OB stars is to develop an empirical relationship between 2um spectral features of these massive stars and their stellar temperature and luminosity. We find the system of lines between 2.0 and 2.2um is particulary good for differentiating the early- and mid-O type stars. In the late-O and early-B stars, differentiation becomes more difficult, as the features show only moderate changes. We have developed a spectral classification system for the K band to be used to estimate effective temperatures of O and early-B stars. We demonstrate that K-band spectroscopy is superior in estimating the temperature of hot, luminous stars than the traditional methods of using infrared or even optical photometric colors alone. The only requirements are that adequate resolution (R>1000) and signal-to-noise (S/N~70) be achieved. With our classification system, stars behind large amounts of visible extinction, such as young, heavily reddened H II regions throughout our Galaxy, may be identified and studied for the first time through 2um spectroscopy. Emission lines are commonly seen in the K-band spectra of supergiant stars, however, the OBN supergiants, which have a higher ratio of some processed materials at their surface, may be more likely to show line emission, especially the He I singlet transition at 2.058um. This has led us to propose an evolutionary scenario for some of the Galactic center He I emission-line stars, which evokes rotational mixing (Maeder 1987A&A...178..159M; Langer 1992A&A...265L..17L) to explain both the strong line emission and high luminosity of these mysterious sources. We have compared our spectroscopic database with the most recent stellar atmosphere models. We are encouraged by the good match between the model line profiles at 2um of Schaerer et al. (1996A&A...312..475S) and those observed in OB stars. Finally, we include a thorough discussion of the observational and reduction methods employed to obtain the spectra shown in this atlas for the benefit of those wishing to obtain similar, classification-quality, near-infrared spectra.
Stars in 2 micron spectral atlas Star Star number Note that HD 47129 is also known as Plaskett's Star. Bagnuolo, Gies & Wiggs (1992ApJ...385..708B) show it to be a pair of supergiants. --- FITSfile Eight-character name for data files The spectrum is stored in FITS format as file: fits/FITSfile.fit --- Sp Optical spectral type --- u_Sp A colon indicates Sp is uncertain --- r_Sp Reference to optical spectral type Reference to the optical spectral type. W72 Walborn (1972AJ.....77..312W) W73 Walborn (1973AJ.....78.1067W) MT Massey & Thompson (1991AJ....101.1408M) C74 Conti (1974ApJ...187..539C) Mth Mathys (1988A&AS...76..427M) C71 Conti & Alschuler (1971ApJ...170..325C) W76 Walborn (1976ApJ...205..419W) M55 Morgan, Code, & Whitford (1955ApJS....2...41M) WF Walborn & Fitzpatrick (1990PASP..102..379W) L Lennon, Dufton, & Fitzsimmons (1992A&AS...94..569L) BS Bright Star Catalogue, Hoffleit (1982, See Cat. <V/50>) S SIMBAD database J93 Jones et al. (1993ApJ...411..323J) GS Garmany & Stencil (1992A&AS...94..211G) vP van Paradijs (1994, in X-ray Binaries, ed. Lewin, van Paradijs & van den Heuvel, p. 536) HP Howarth & Prinja (1989ApJS...69..527) G77 Garrison, Hiltner, & Schild (1977ApJS...35..111G) Note on Detector: CRSP KPNO Cryogenic Infrared Spectrometer FSPEC Steward Observatory Infrared Spectrometer IRS CTIO Infrared Spectrometer OSIRIS Ohio State Infrared Imaging Spectrometer --- Detector Detector used for the observation --- SpRes Spectral resolution, Lambda / dLambda --- DateObs Date of observation (MM/YY) "MM/YY" SpK K-band spectral type --- Notes Notes, mostly alternate identifications --- table1.tex AASTeX version of table1.dat Patricia Bauer CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 09-Oct-96 J_ApJS_107_281.xml Redshift distribution of galaxies in the southern Milky way region 210{deg}<l<360{deg} and |b|<15{deg}. J/ApJS/107/521 J/ApJS/107/521 Galaxies redshifts, 210<l<360, |b|<15 Redshift distribution of galaxies in the southern Milky way region 210{deg}<l<360{deg} and |b|<15{deg}. N Visvanathan T Yamada Astrophys. J. Suppl. Ser. 107 521 1996 1996ApJS..107..521V III/40 : Spectral Survey of Southern Milky Way (Loden+ 1976) VII/140 : Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91) II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) J/A+AS/104/529 : IRAS galaxies behind the Milky Way (Takata+ 1994) J/MNRAS/287/472 : Southern Milky Way galaxies velocities (Di Nella+ 1997) Galaxy catalogs Infrared sources Redshifts cosmology: observations galaxies: distances and redshifts We have carried out a redshift survey of an IRAS flux-limited (f_60_>0.6) galaxy sample behind the southern Milky Way, 210{deg}<l<360{deg} at |b|<15{deg}. The survey includes redshifts for 951 galaxies, ~500 of which are new. Of these 951 galaxies, 462 are in the zone 5{deg}<b<15{deg} and 353 are in the zone -15{deg}<b<-5{deg}. Though the innermost region of the Milky Way (|b|=5{deg}) remains opaque except in the longitude near 240, the detected galaxies show a high degree of completeness (~70%) in the zones 5{deg}<b<15{deg} and -15{deg}<b<-5{deg}. The cone diagrams exhibiting the detailed distribution of IRAS galaxies in the region 210{deg}<l<360{deg}, |b|<15{deg} shows two clusters in the Puppis region (l=240{deg}, b=-7{deg}, v=2400km/s; l=245{deg}, b=-5{deg}, v=7500km/s), the A3627 cluster (l=325{deg}, b=-7{deg}; v=4500km/s), the S4 cluster (l=280{deg}, b=7{deg}; v=5500km/s), and a possible void at l=245{deg}, v=3000km/s. The region 270{deg}<l<350{deg} is dominated by overdensity of galaxies representing the extension of the Hydra-Centaurus complex in the positive latitudes and the Pavo-Indus complex in the negative latitudes. A velocity histogram of galaxies in the GA region 290{deg}<l<350{deg}, |b|<15{deg}. reveals a substantial overdensity of galaxies in the velocity range 2400-5000km/s. The centroid of this overdensity is located at 4000km/s. The broad increased density of galaxies seen in our data corresponds with the distant concentration seen at 4500km/s in the supergalactic plane survey that covers the same longitude range like ours in l, but a larger range in latitude b (-30{deg} to -10{deg} and +10{deg} to +45{deg}). This lends support to the idea that the overdensity extends all the way from the Centaurus-Hydra complex (l=302{deg}, b=+22{deg}) in the north to the major concentration of the Pavo-Indus supercluster (l=332{deg}, b=-24{deg}) in the south, through the Milky Way. We conclude that the peak of the overdensity responsible for the peculiar velocity field in the local region is possibly situated in the Milky Way itself.
List of galaxies behind the southern Milky Way IRAS IRAS-PSC (Cat. <II/125>) name --- Typo Correction, see "History" section below --- GLON Galactic longitude deg GLAT Galactic latitude deg cz Heliocentric redshift km/s n_cz Note on cz number=1 S: radial velocity data kindly provided by W. Saunders. a: Radial velocity data kindly provided by K. B. Fisher. b: Radial velocity data listed in Yamada et al. (1993ApJS...89...57Y) c: Radial velocity taken from SIMBAD. --- S60um Flux density at 60{mu}m Jy Bmag B magnitude mag n_Bmag Note on Bmag number=2 c: Blue magnitudes taken from SIMBAD Unfootnoted B magnitude values are estimated roughly from size for galaxies in Yamada et al. (1993ApJS...89...57Y). Magnitudes of galaxies provided by K. B. Fisher are not available. --- James Marcout, Patricia Bauer CDS 1998 May 12 UNKNOWN UNKNOWN Prepared via OCR at CDS. * 30-Sep-1998: 7 errors in the paper (indicated by an '*' in Typo column of table1.dat) were detected by H. Andernach (heinz@astro.ugto.mx) and corrected. J_ApJS_107_521.xml Parameters of 2447 southern spiral galaxies for use in the Tully-Fisher relation J/ApJS/107/97 J/ApJS/107/97 Parameters of 2447 southern spirals Parameters of 2447 southern spiral galaxies for use in the Tully-Fisher relation D S Mathewson V L Ford Astrophys. J. Suppl. Ser. 107 97 1996 1996ApJS..107...97M Galaxies, photometry Morphology Redshifts Rotational velocities galaxies: distances and redshifts galaxies: kinematics and dynamics galaxies: photometry surveys I-band luminosities, rotational velocities, and redshifts of 1092 spiral galaxies have been measured by CCD photometry and Halpha spectroscopy using the 1m and 2.3m telescopes at Siding Spring Observatory, respectively. The results are tabulated. Luminosity profiles and Halpha rotation curves are given for the galaxies. When these results are combined with similar data for 1355 spiral galaxies published previously (Mathewson, Ford, & Buchhorn, hereafter Paper I, 1992ApJS...81..413M), it provides a large, uniform, and unique data set with which to measure, via the Tully-Fisher relation, the peculiar velocities of galaxies in the local universe to a distance of 11,000km/s (Mathewson & Ford, in Proc. Heron Island Workshop on Peculiar Velocities in the Universe). Taking advantage of the opportunity for publishing this data in machine-readable form, in the CD-ROM, we have also published similar data for the 1355 galaxies in Paper I.
Physical parameters, photometric and velocity data for survey galaxies Name Galaxy identification number Galaxy identification number; for galaxies south of -17.5 deg; it is the ESO-Uppsala Catalog (Cat. <VII/34>) number, and for galaxies north of -17.5 deg, it is either the UGC number (Cat. <VII/26>, the NGC (Cat. <VII/1>) or IC designation, or the MCG (Cat. <VII/62>) number. --- RAh Right ascension, 1950 h RAm Right ascension, 1950 min RAs Right ascension, 1950 s DE- Declination sign --- DEd Declination, 1950 deg DEm Declination, 1950 arcmin DEs Declination, 1950 arcsec GLon Galactic longitude deg GLat Galactic latitude deg SGL Supergalactic longitude deg SGB Supergalactic latitude deg Class Classification in the Hubble system --- Type Morphological type, +3 for Sb to +8 for Sd --- aESO Major axis diameter from various catalogs arcmin a Major axis diameter Major and minor axes diameters of the I = 23.5 mag/arcsec2 isophote. arcmin b Minor axis diameter arcmin i Inclination of optical disk Inclination of the optical disk computed from the average of axial ratios of the ellipses of surface brightness I = 22.5, 23.0, and 23.5 mag/arcsec2, following Bothun et al. (1985ApJS...57..423B). deg PA Position angle of the major axis Position angle of the major axis, which is an average of the position angles of the major axes of the ellipses of surface brightness I = 22.5, 23.0, and 23.5 mag/arcsec2 or the P.A. given in the ESO-Uppsala Catalog. deg D0 Face-on diameter Face-on diameter D(0) computed using the relation log D(0) = log(a) - 0.235 log(a/b) + 0.09 Aext where Aext = the absorption in our Galaxy, and the maximum value of a/b is 5 (cf. de Vaucouleurs, de Vaucouleurs, & Corwin 1976, Cat. <VII/112>). arcmin Aext Extinction in our Galaxy in I magnitudes The extinction in our Galaxy in I magnitudes. This has been calculated following Burstein & Heiles (1978ApJ...225...40B). The relation used is Aext=4.05x10^-4F(HI)-0.06. F(HI) is the integrated "zero-velocity" H I flux density in Jy km/s, measured with the 64 m Parkes radio telescope in the direction of each galaxy. The extinction in I is taken to be 42% of that in B. mag Aint Internal extinction in I magnitudes Internal extinction in a galaxy in I magnitudes. The corrections prescribed by Tully & Fouque, (1985ApJS...58...67T), were used to yield "face-on" magnitudes. The extinction in I is taken to be 42% of that in B. mag Kz K correction in I magnitudes K-correction in I magnitudes. The values were taken from Schneider et al. 1983ApJ...264..337S. mag It Total I magnitudes mag Itc Total I magnitudes corrected for extinction Total I magnitudes corrected for internal and external extinction and K dimming: Itc=It-Aext-Aint-Kz. mag ISB Integrated surface brightness Integrated surface brightness in I magnitudes/arcsec2: ISB=c_D(0)+5logD(0)+2.5log(pi) where Ic_D(0)=I_D(0)-Aext-Aint-Kz and I_D(0) are measured from the GASP output files. mag/arcsec2 Vopt Heliocentric systemic velocity, optical Heliocentric systemic velocity taken as the arithmetic mean of the maximum and minimum velocities of the optical rotation curve. km/s Vradio Heliocentric systemic velocity, radio Heliocentric systemic velocity taken as the arithmetic mean of the velocities where the H I profile falls to 50% of the mean of the highest channels in each half of the profile. km/s DVopt Diff. of max and min optical rotation Half the difference between the maximum and minimum values of the optical rotation curve, corrected for relativistic effects, i.e., divided by 1+z. km/s DV50 Diff. of H I profile at 50% intensity Half the widths of the H I profile between points where the intensity falls to 50% of the highest channels in each half of the profile and points corrected for relativistic effects. km/s e_DV50a First uncertainty in DV50 measurement Uncertainties in the measurement of DV50. These errors were calculated by perturbing the 50% level by the rms noise in the spectrum and measuring the amount by which the width changed. km/s e_DV50b Second uncertainty in DV50 measurement km/s DV20 Diff of H I profile at 20% intensity Same as DV50, but for the 20% level. km/s e_DV20a First uncertainty in DV20 measurement Same as e_DV20, but for the 20% level. Sometimes due to noise spikes, unrealistic error values were recorded. In this case, the the error fields may be blank. km/s e_DV20b Second uncertainty in DV20 measurement km/s Vrot Maximum rotation velocity of spiral galaxy Maximum velocity of rotation of the spiral galaxy, obtained by dividing DVopt by sin i. When there was only a radio measurement, DV50 was converted to DVopt using the algorithm DVopt = 1.03 DV50 - 11. km/s u_Vrot Vrot calculated by alternate method The colons after 20 of the Vrot entries indicate that the rotational velocities were derived from radio measurements by M. Haynes and R. Giovanelli, and converted to DVopt using the algorithm DVopt = 1.10 DV50 - 27. --- FHI H I flux density integral H I flux density integral corrected for beam effects. Jy.km/s rms rms noise mJy S/N Peak signal divided by rms noise --- Vcmb Heliocentric systemic velocity in CMB frame Heliocentric systemic velocity converted to the cosmic microwave background (CMB) frame of reference. If both Vopt and Vradio are given, Vopt is used, otherwise Vradio. There is no significant difference between the two values. km/s Vlg Heliocentric velocity in Local Group frame The same as Vcmb, except heliocentric velocities are converted to the frame of the Local Group. km/s CDS 1997 Feb 03 AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 04-Nov-96 J_ApJS_107_97.xml Deep imaging of the field of the high-redshift radio source 4C 23.56 J/ApJS/109/367 J/ApJS/109/367 4C 23.56 field deep imaging Deep imaging of the field of the high-redshift radio source 4C 23.56 G P Knopp K C Chambers Astrophys. J. Suppl. Ser. 109 367 1997 1997ApJS..109..367K Galaxies, radio Photometry, infrared galaxies: individual (4C 23.56) galaxies: photometry galaxies: structure infrared: galaxies radio continuum: galaxies We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'>4mag in the field, including two with I-K'>6mag.
Photometry of 4C 23.56 field sources Seq Source sequential number --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec l_U'mag Limit flag on U'mag --- U'mag U' magnitude (3402{AA}) mag e_U'mag rms uncertainty on U'mag mag n_U'mag Note on U'mag number=1 We abbreviate the notes to waveband measurements as s = saturated o = obscured in the wings of a bright source and thus not identified f = failed to meet selection criteria --- l_NB Limit flag on NB --- NB Narrow band magnitude (4229{AA}) in AB magnitude number=2 In the AB-magnitude system, any object with a flat spectrum (F_{nu} prop. to {nu}^0^) has the same magnitude, independent of passband: m_AB_=-2.5log(f_{nu}_) - 48.59 mag e_NB rms uncertainty on NB in AB magnitude number=2 In the AB-magnitude system, any object with a flat spectrum (F_{nu} prop. to {nu}^0^) has the same magnitude, independent of passband: m_AB_=-2.5log(f_{nu}_) - 48.59 mag n_NB Note on NB number=1 We abbreviate the notes to waveband measurements as s = saturated o = obscured in the wings of a bright source and thus not identified f = failed to meet selection criteria --- l_Vmag Limit flag on Vmag --- Vmag V magnitude (5457{AA}) mag e_Vmag rms uncertainty on Vmag mag n_Vmag Note on Vmag number=1 We abbreviate the notes to waveband measurements as s = saturated o = obscured in the wings of a bright source and thus not identified f = failed to meet selection criteria --- l_Imag Limit flag on Imag --- Imag I magnitude (8300{AA}) mag e_Imag rms uncertainty on Imag mag n_Imag Note on Imag number=1 We abbreviate the notes to waveband measurements as s = saturated o = obscured in the wings of a bright source and thus not identified f = failed to meet selection criteria --- l_K'mag Limit flag on K'mag --- K'mag K' magnitude (21100{AA}) mag e_K'mag rms uncertainty on K'mag mag n_K'mag Note on K'mag number=1 We abbreviate the notes to waveband measurements as s = saturated o = obscured in the wings of a bright source and thus not identified f = failed to meet selection criteria --- Class Classification number=3 Our tentative object classifications are abbreviated as follows: FS = field star UG = unidentified galaxy E = elliptical S = spiral Im = irregular RG = 4C 23.56 --- James Marcout, Patricia Bauer CDS 1997 Oct 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_109_367.xml The Kitt Peak galaxy redshift survey with multicolor photometry: basic data wJ/ApJS/109/45 wJ/ApJS/109/45 Kitt Peak galaxy redshift survey The Kitt Peak galaxy redshift survey with multicolor photometry: basic data J A Munn D C Koo R G Kron S R Majewski M A Bershady J J Smetanka Astrophys. J. Suppl. Ser. 109 45 1997 1997ApJS..109...45M Galaxies, photometry Redshifts astrometry cosmology: observations galaxies: distances and redshifts galaxies: photometry surveys Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_<=18.5 and R_F<=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_<=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_>20.
SA 68 00 17 28 +15 53 12 Lynx 2 08 45 07 +44 35 47 SA 57 13 08 +29 24 Her 1 17 20 13 +49 55 30
Multiaperture Masks Field Field number=1 A: SA 57 B: SA 68 C: Her 1 D: Lynx 2 --- Seq Sequence number, by which it is identified throughout the paper --- Aper Type of aperture (Holes or Slits) --- KPNO KPNO serial number --- Ident Authors' identifier --- RAh Right ascension of mask center (1950 equinox) h RAm Right ascension of mask center (1950 equinox) min RAs Right ascension of mask center (1950 equinox) s DE- Declination sign --- DEd Declination of mask center (1950 equinox) deg DEm Declination of mask center (1950 equinox) arcmin DEs Declination of mask center (1950 equinox) arcsec Run Observing runs during which the mask was observed number=2 The mask was originally created for the first run in the list. If the first run is parenthesized, then it was not observed during that run, although it was created for that run. --- Texp Total exposure time s Target List of special targets --- *Catalog MKK97 Identifying serial number number=1 Objects in fields SA57, SA68, Her1, and Lynx2 begin with the digit 1, 2, 3, and 4, respectively. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec RFmag Total R_F_ (R_F_ approx. (V+R)/2) magnitude number=2 In SA57 and SA68, this means the magnitude within a circular aperture of radius 2*r1. In Her1 and Lynx2, this means the FOCAS total magnitude (magnitude within an area at least twice the size of that contained within the detection isophote). mag U-BJ U-B_Johnson_ color number=3 In SA57 and SA68, the colors are derived from magnitudes measured in a circular aperture of radius 2*r1. In Her1 and Lynx2, the colors are derived from magnitudes measured in a circular aperture of radius 2 arcsec. The 5 off-scale values (MKK97= 103357, 103341, 213807, 217739, 316656) reflect the fact that the photometry for individual objects can be wrong due to plate defects or whatever. They clearly indicate that the photometry in at least one band for that object is questionable. mag BJ-RF B_Johnson_-R_F_ color mag RF-IN R_F_-I_N_ color (I_N_ approx. Kron-Cousins I) mag z Redshift number=4 Objects with a redshift of 0.0000 were morphologically classified as galaxies, but spectroscopically found to be stars. --- q_z Redshift quality number=5 q = min[6, min(1, Ndef) + 2 Ndef + Nprob], where Ndef and Nprob are the number of definite and probable features, respectively. --- r_z The sources of the redshift number=6 (A---OO): multi-hole or multi-slit spectrum from the specified mask (cross-reference to column 1 in Table 5) (a---z): long-slit or multi-fiber spectrum from the specified observing run (cross-reference to column 1 in Table 3) (1) Spinrad, 1980, private communication; (2) Turner, 1980, private communication; (3) Based on observations obtained at the W. M. Keck Observatory, which is operated jointly by the California Institute of Technology and the University of California. --- Ns The number of galaxies, brighter than this galaxy in R_F_ and within the field-of-view of this galaxy's primary mask, for which no spectra were ever obtained and no other redshifts exist. --- Nb The number of galaxies, brighter than this galaxy in R_F_ and part of the statistical sample defined by this galaxy's primary mask, which have been observed spectroscopically, but which lack definite redshifts (q>2). number=7 If this value is -1, then all galaxies brighter than this galaxy in F which are within the field-of-view of this galaxy's primary mask have q>2 redshifts. --- Note Notes number=8 B: special target of the mask, selected as a bright galaxy; C: special target of the mask, selected as a member of a cluster of galaxies; J: special target of the mask, selected as a member of a faint J-selected sample; N: special target of the mask, selected as a candidate NELG; R: special target of the mask, selected as a radio source; U: special target of the mask, selected as a UV-excess source; X: not targeted by the mask, but accidentally fell within a slitlet or slit targeted at a different object. --- James Marcout, Patricia Bauer CDS 1998 Feb 23 Jeff Munn <jam@nofs.navy.mil> wJ_ApJS_109_45.xml Main-line OH observations of the Arecibo set of OH/IR stars J/ApJS/109/489 J/ApJS/109/489 OH observations of Arecibo OH/IR stars Main-line OH observations of the Arecibo set of OH/IR stars B M Lewis Astrophys. J. Suppl. Ser. 109 489 1997 1997ApJS..109..489L J/ApJS/89/189 : IRAS PSC new OH/IR stars. III. (Chengalur+ 1993) J/ApJS/93/549 : Arecibo 1612 MHz survey supplement (Lewis 1994) Infrared sources Masers Radio lines Spectroscopy infrared: stars masers radio lines: stars stars: AGB and post-AGB surveys The Arecibo 1612MHz survey of a complete sample of color-selected IRAS sources with 25{mu}m fluxes S(25)>2 Jy detected 393 OH/IR stars. A complementary 1667 and 1665MHz OH survey of these objects is presented here. Main-line masers have been detected in 238 surveyed objects: 18 exhibit only 1665MHz emission, 220 exhibit 1667MHz masers, and 119 exhibit both. The main lines were not detected in 159 objects.
Main-line peak data IRAS IRAS name --- Date Date in the form "yyddd" number=1 Dates of observation are given in the form yyddd, e.g., 89220 is the 220th day of 1989. "YYDDD" Note Note on circular polarisation number=2 LC: Left circular RC: Right circular --- V1667 Velocity of the 1667MHz feature km/s u_V1667 Uncertainty flag on V1667 --- l_I1667 Limit flag on I1667 --- I1667 Unsmoothed peak intensity of the 1667MHz feature mJy u_I1667 Uncertainty flag on I1667 --- V1665 Velocity of the 1665MHz feature km/s l_I1665 Limit flag on I1665 --- I1665 Unsmoothed peak intensity of the 1665MHz feature mJy u_I1665 Uncertainty flag on I1665 --- Main-line nondetections among the Arecibo OH/IR stars IRAS IRAS name --- m_IRAS Multiplicity index on IRAS --- Patricia Bauer CDS 1998 Apr 02 UNKNOWN UNKNOWN Copied form ApJS electronic version J_ApJS_109_489.xml Redshift survey of galaxies around a selected sample of compact groups. J/ApJS/110/1 J/ApJS/110/1 Galaxies around HCGs Redshift survey of galaxies around a selected sample of compact groups. R R De Carvalho A L B Ribeiro H V Capelato S E Zepf Astrophys. J. Suppl. 110 1 1997 1997ApJS..110....1D VII/85 : Hickson Compact Groups of Galaxies (Hickson 1982) Clusters, galaxy Radial velocities galaxies: clusters: general galaxies: distances and redshifts methods: statistical We report the results of a spectroscopic survey of faint galaxies in the regions surrounding Hickson compact groups. Our sample is composed of 17 groups within 9000km/s. The spectra were taken at the prime focus of the Tololo 4m telescope, using the ARGUS fiber-fed spectrograph. From these observations, redshifts were determined for the faint galaxies previously identified by de Carvalho, Ribeiro & Zepf (1994ApJS...93...47D) in the surroundings of the groups. Statistical methods were applied to the resultant catalog in order to determine the kinematical structure of each group. This analysis confirms the idea that the Hickson sample of compact groups contains a wide variety of projection and dynamical configurations. Our results demonstrate the necessity of new spectroscopic surveys around compact groups in order to assess their complete velocity distribution.
Catalog of galaxies around HCGs Name Name according to dCAZ94 (1994ApJS...93...47D) --- m_Name Multiplicity index on Name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) DEs is listed to more digits than would correspond to the actual precision of positions (0.2"-0.3"). arcsec Bmag Total B magnitude mag RV Radial velocity km/s e_RV rms uncertainty on RV km/s R R parameter (Tonry & Davis, 1979AJ.....84.1511T) --- Lines Emission lines identified --- James Marcout, Patricia Bauer CDS 1997 Oct 26 UNKNOWN UNKNOWN Prepared via OCR at CDS and independently by H.Andernach (Guanajuato). We thank H. Andernach for his comparison of both results and his proofreading. J_ApJS_110_1.xml A Catalog of Morphological Types in 10 Distant Rich Clusters of Galaxies J/ApJS/110/213 J/ApJS/110/213 Morphological Types in 10 Distant Rich Clusters A Catalog of Morphological Types in 10 Distant Rich Clusters of Galaxies I Smail A Dressler W J Couch R S Ellis A Oemler Jr. H Butcher R M Sharples Astrophys. J. Suppl. Ser. 110 213 1997 1997ApJS..110..213S Clusters, galaxy Galaxy catalogs catalogs galaxies: clusters: general galaxies: structure The catalogs are presented in ASCII tables, along with FITS images of the HST observations and Postscript versions of the plates from the printed paper. We present catalogs of objects detected in deep images of 11 fields in 10 distant clusters obtained using WFPC-2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry and basic morphological information on ~9000 objects in the fields of the 10 clusters. For a brighter subset of 1857 objects in these areas, we provide more detailed morphological information.
HST
Cluster parameters Cluster Cluster (as in other tables) --- Name Cluster designation --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec PAV3 Position angle of field deg z Cluster redshift --- F450W Exposure time with F450W filter ks F555W Exposure time with F555W filter ks F702W Exposure time with F720W filter ks F814W Exposure time with F814W filter ks Lx X-ray luminosity (0.3-3.5keV) 10+37W sVel Velocity dispersion km/s e_sVel Mean error on sVel km/s Scale assuming Ho=100km/s/Mpc kpc/arcsec E(B-V) Extinction mag mu1 Surface brightness limit mag/arcsec+2 Object Catalog Cluster Cluster field (see table1.dat) --- ID Object Number in cluster IDs starting 2000 denote objects lying on the PC chip; those starting 3000 are "additional" objects lying on the WFC --- Xpos X centroid on frame pix Ypos Y centroid on frame pix mag1.0 1.0arcsec diameter red aperture magnitude the parameter is F814W for clusters a,c,e,h,j,k, and F702W for the clusters b,d,f,g,i mag e_mag1.0 Mean error on mag1.0 mag isomag Isophotal magnitude above detection isophote mag e_isomag Mean error on isomag mag bestmag Optimal measure of total magnitude variable-diameter aperture magnitude measured in an elliptical aperture of major axis 2.5rK, unless Flags=1 occurred in which case the "corrected" isophotal magnitude is used (Bertin & Arnouts, 1996A&AS..117..393B) mag e_bestmag Mean error on bestmag mag Area Isophotal area above detection isophote pix rK Kron radius pix a Second-order moment along major axis pix b Second-order moment along minor axis pix theta Orientation of major axis theta is defined counter-clockwise from the positive X-axis deg mu(thresh) Detection threshold mag/arcsec2 mu(max) Peak surface brightness mag/arcsec2 Sky Background level (DN) --- FWHM from Gaussain fit pix P(star) Star-galaxy classification classifier using neural-net weights: 0.0=galaxy, 1.0=star --- C1 Concentration index C1 represents the fraction of an object's light contained in the central 30% of its area as measured in an ellipse aligned with the object and having the same axial ratio (see Abraham et al., 1994ApJ...432...75A). C1 is a measure of how centrally peaked an object is. --- C2 Constrast index C2 measures the fraction of an object's light contained in the brightest 30% of its pixels. C2 provides a measure similar to C1, but without requiring the light to be centrally concentrated --- Flags Error flags 1: bright neighbors may bias magnitude estimate; 2: originally a blend; 4: saturated; 8: object truncated by frame boundary; 16: incomplete aperture photometry; 32: incomplete isophotal photometry; 64: memory overflow during deblending; 128: memory overflow during extraction. --- ci1.0 Color measured in a 1.0" diameter aperture Only for those fields with color information: F555W-F814W for clusters a,e,h,j,k ; F450W-F814W for cluster c. mag e_ci1.0 Mean error on ci1.0 mag Morphology Catalog Cluster Cluster field (see table1.dat) --- ID Object Number in cluster IDs starting 2000 denote objects lying on the PC chip; those starting 3000 are "additional" objects lying on the WFC --- DG Designation in Dressler (1992ApJS...78....1D) Nonexhaustive cross identification of objects against the catalogs in Dressler & Gunn (1992ApJS...78....1D), for the clusters Cl 0024+16, Cl 0939+47, Cl 0303+17, 3C 295, Cl 1601+42, and Cl 0016+16 --- bestmag Optimal measure of total red magnitude the parameter is F814W for clusters a,c,e,h,j,k, and F702W for the clusters b,d,f,g,i mag Asym Asymetry parameter variable-diameter aperture magnitude measured in an elliptical aperture of major axis 2.5rK, unless Flags=1 occurred in which case the "corrected" isophotal magnitude is used (Bertin & Arnouts, 1996A&AS..117..393B) --- MType Hubble class The standard Hubble classification scheme (E, S0, Sa, Sb ) with the addition of the following: D, cD, Morgan type D or cD galaxy; E/S0 or S0/E, cannot distinguish E or S0; X, compact object (likely nonstellar but too compact to see structure); *, stellar image; ?, unclassifiable. --- TType =-99 Numeric T-type --- D =-99 Disturbance index Disturbance index: 0, normal; 1, moderate asymmetry; 2, strong asymmetry; 3, moderate distortion; 4, strong distortion; -99, undefined. --- Int Interpretation of disturbance Interpretation of disturbance classes: M, merger; I, tidal interaction with neighbor; T, tidal feature; C, chaotic; !.remarkable. --- Comment Description of object morphology --- imageva.fit Reduced F555W WFPC-2 frame of A370 Field 2 imageia.fit Reduced F814W WFPC-2 frame of A370 Field 2 imagerb.fit Reduced F702W WFPC-2 frame of Cl 1447+23 imagebc.fit Reduced F450W WFPC-2 frame of Cl 0024+16 imageic.fit Reduced F814W WFPC-2 frame of Cl 0024+16 imagerd.fit Reduced F702W WFPC-2 frame of Cl 0939+47 imageve.fit Reduced F555W WFPC-2 frame of Cl 0939+47 F2 imageie.fit Reduced F814W WFPC-2 frame of Cl 0939+47 F2 imagerf.fit Reduced F702W WFPC-2 frame of Cl 0303+17 imagerg.fit Reduced F702W WFPC-2 frame of 3C 295 imagevh.fit Reduced F555W WFPC-2 frame of Cl 0412-65 imageih.fit Reduced F814W WFPC-2 frame of Cl 0412-65 imageri.fit Reduced F702W WFPC-2 frame of Cl 1601+42 imagevj.fit Reduced F555W WFPC-2 frame of Cl 0016+16 imageij.fit Reduced F814W WFPC-2 frame of Cl 0016+16 imagevk.fit Reduced F555W WFPC-2 frame of Cl 0054-27 imageik.fit Reduced F814W WFPC-2 frame of Cl 0054-27 plate1a.ps Postscript version of Plate 1a (A370 Field 2) plate1b.ps Postscript version of Plate 1b (Cl 1447+23) plate1c.ps Postscript version of Plate 1c (Cl 0024+16) plate1d.ps Postscript version of Plate 1d (Cl 0939+47) plate1e.ps Postscript version of Plate 1e (Cl 0939+47 F2) plate1f.ps Postscript version of Plate 1f (Cl 0303+17) plate1g.ps Postscript version of Plate 1g (3C 295) plate1h.ps Postscript version of Plate 1h (Cl 0412-65) plate1i.ps Postscript version of Plate 1i (Cl 1601+42) plate1j.ps Postscript version of Plate 1j (Cl 0016+16) plate1k.ps Postscript version of Plate 1k (Cl 0054-27) Francois Ochsenbein CDS 1998 Jun 04 UNKNOWN UNKNOWN * 07-May-1997: tabular data as a set of 22 FITS files on AAS CD-ROM series, Volume 8, 1997, directory /volume8/apjs/inpress/smail (Lee Brotzman) * 04-Jun-1998: tables reformatted and merged into 3 tables at CDS (F. Ochsenbein) J_ApJS_110_213.xml Molecular clouds in Cepheus and Cassiopeia. J/ApJS/110/21 J/ApJS/110/21 Molecular clouds in Cepheus and Cassiopeia Molecular clouds in Cepheus and Cassiopeia. Y Yonekura K Dobashi A Mizuno H Ogawa Y Fukui Astrophys. J. Suppl. Ser. 110 21 1997 1997ApJS..110...21Y Carbon monoxide Interstellar medium ISM: clouds ISM: molecules ISM: structure radio lines: ISM stars: formation surveys A large-scale ^13CO(J=1-0) survey for nearby molecular clouds was performed toward the Cepheus and Cassiopeia regions (100{deg}<l<130{deg} and -10{deg}<b<20{deg}) with the velocity coverage of -40<V_LSR_<+20km/s by using the two 4m millimeter-wave telescopes at Nagoya University. An area of 866 square degrees was covered at an 8' grid spacing with a 2.7' beam, and 48750 positions were observed. Significant ^13^CO emission (>=1.8K.km/s=3{sigma}) is detected at 1015 positions. On the basis of the ^13^CO data, 188 distinct ^13^CO clouds are identified whose total mass is 1.0x10^5^M_{sun}_. Physical properties of the ^13^CO clouds such as molecular column densities, sizes, and masses are derived for each cloud. Astronomical objects associated with the ^13^CO clouds were searched for in the literature: 10 H II regions, eight reflection nebulae, 23 T Tauri type stars, 28 molecular outflows, and 125 IRAS point sources selected as candidates for protostars are likely to be associated with the ^13^CO clouds.
A catalog of ^13^CO clouds [YDM97]CO Sequential number ([YDM97] CO NNN in Simbad database) --- Note Note number=1 b and c indicates the second and third values of the observed properties set (T*_R_, {delta}Vc and V_lsr_c) --- Cloud Cloud name --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (1950) number=2 Peak positions of the ^13^CO clouds h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) number=2 Peak positions of the ^13^CO clouds deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec TR* Temperature T^*^_R_(^13^CO) K DV FWHM line width {DELTA}V(^13^CO) km/s Vlsr LSR velocity km/s IntI Integrated intensity K.km/s tau Peak optical depth of the ^13^CO line measured at the peak positions of the ^13^CO clouds cm-2 N(H2) H_2_ molecular column density at the peak position 10+21cm-2 size1 Size number=3 Sizes of the ^13^CO clouds measured at 1.8K.km/s contours in Fig.1 (3{sigma}) arcmin --- --- size2 Size number=3 Sizes of the ^13^CO clouds measured at 1.8K.km/s contours in Fig.1 (3{sigma}) arcmin Dist Adopted distance pc n_Dist Note on Dist number=4 Distances of these clouds were decided by the first step --- Mcloud Molecular mass of the ^13^CO cloud solMass r_Dist References to the adopted distances number=5 The references are in the ref.dat file --- Characteristics of cloud groups Group C: Close group D: Distant Group; A: clouds in Perseus Arm --- [YDM97]GCl Sequential number ([YDM97] GCl NN in Simbad database) --- GLONmin Minimum galactic longitude deg GLONmax Maximum galactic longitude deg GLATmin Minimum galactic latitude deg GLATmax Maximum galactic latitude deg Vmin Minimum V_LSR_ km/s Vmax Maximum V_LSR_ km/s Dist Adopted distance of the subgroup pc Mass Total molecular mass of the subgroup solMass Ncloud Number of component clouds identified in S3.2. --- AssObj Associated objects --- r_Dist References for adopted distances in refs.dat --- References Ref References number --- Aut Author's name --- BibCode Simbad bibcode --- Com Comment --- James Marcout, Patricia Bauer CDS 1998 May 04 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_110_21.xml Faust observations of ultraviolet sources toward the Virgo cluster J/ApJS/111/143 J/ApJS/111/143 Virgo cluster ultraviolet sources Faust observations of ultraviolet sources toward the Virgo cluster N Brosch L Formiggini E Almoznino T Sasseen M Lampton S Bowyer Astrophys. J. Suppl. Ser. 111 143 1997 1997ApJS..111..143B VII/48 : Catalogue of middle UV photometry of Virgo cluster galaxies J/ApJS/96/461 : Far-UV Point Sources (Bowyer+ 1995) Clusters, galaxy Photometry, UBV Photometry, ultraviolet galaxies: clusters: individual (Virgo) galaxies: fundamental parameters ultraviolet: galaxies ultraviolet: stars We analyze three UV images covering a ~100 square degree field toward the Virgo cluster, obtained by the FAUST space experiment. We detect 191 sources to a signal-to-noise ratio of 4.4 and identify 94% of them. Most sources have optical counterparts in existing catalogs, and about half are identified as galaxies. Some sources with no listed counterpart were observed at the Wise Observatory. We present the results of low-resolution visible spectrophotometry and discuss the foreground 101 stellar sources and the 76 detected galaxies, both in the cluster and in the foreground or background. We derive conclusions on star formation properties of galaxies and on the total UV flux from discrete and diffuse sources in the cluster. We test for the presence of intracluster dust, determine the clustering properties of UV emitting galaxies, and derive the UV luminosity function of Virgo galaxies.
FAUST
Detected FAUST sources in the Virgo images ID Identification number --- n_RAh Note number=1 An * indicates objects for which the coordinates were calculated from an astrometric solution based in bright, well-identified stellar images. --- RAh Right ascension h RAm Right ascension min RAs Right ascension s DEd Declination deg DEm Declination arcmin DEs Declination arcsec UVmag Adopted FAUST UV magnitude number=2 The adopted UV magnitude is the average of the different FAUST measurements. The error is the root mean square of the individual errors. mag e_UVmag rms uncertainty on UVmag mag u_UVmag Uncertainty flag on UVmag number=3 A colon (:) indicates a very large measurement error. --- Nobs Number of observations number=4 Nobs is the number of times a source was observed, i.e., the number of FAUST images in which it appears. --- Ident Proposed identification --- n_Ident Note number=5 The question mark (?) at ID 44, ID 57, and ID 69 indicates that the proposed identification is a bit off the FAUST source. ID 52: The UV source may be a blend of the emission from the galaxy and the HD 108285 (A2) star. ID 155: The three stars near the FAUST source have been observed spectroscopically and identified with late G or K star. The proposed identification is the faint KARA 68181 galaxy marked on the overlays of the PSS. Note that there is a dE galaxy (VCC 1866) a bit far from the FAUST source. ID 164: This source is near the TD-1 26442 from the Extended TD-1 catalog (preprint). On the PSS there is a faint V>15 blue looking candidate 123945+163743 not observed. --- FAUST Entry in FAUST catalog --- --- --- FAUST2 Second entry in FAUST catalog --- --- --- FAUST3 Third entry in FAUST catalog --- Stars toward the Virgo cluster Source Source number --- Name Identification name --- SpType Spectral classification number=1 The spectral classification is mainly from HIC (Cat. <I/196>), in which case the HIC number is marked in Other The stars classified from WiseObs spectra have the note (e) early, or (l) late, according to the appearance or absence of spectral features in our low-resolution spectra. --- l_Vmag Limit flag on Vmag --- Vmag V or B magnitude number=2 The V, B-V and U-B data are from HIC (Cat. <I/196>), or from SAO (Cat. <I/111>) when the star is an SAO object but not a HIC object or from the HD (Cat. <III/135>) catalog if not in either of the two. Seven PG objects have spectral and photometric data from Green et al. (1986, Cat. <II/207>). mag n_Vmag B: B magnitude in Vmag, else V magnitude --- B-V B-V colour index number=2 The V, B-V and U-B data are from HIC (Cat. <I/196>), or from SAO (Cat. <I/111>) when the star is an SAO object but not a HIC object or from the HD (Cat. <III/135>) catalog if not in either of the two. Seven PG objects have spectral and photometric data from Green et al. (1986, Cat. <II/207>). mag U-B U-B colour index number=2 The V, B-V and U-B data are from HIC (Cat. <I/196>), or from SAO (Cat. <I/111>) when the star is an SAO object but not a HIC object or from the HD (Cat. <III/135>) catalog if not in either of the two. Seven PG objects have spectral and photometric data from Green et al. (1986, Cat. <II/207>). mag UVmag FAUST UV magnitude mag u_UVmag Uncertainty flag on UVmag --- e_UVmag rms uncertainty on UVmag mag Other Other Identifications --- Galaxies toward the Virgo cluster-ultraviolet data Source Source number --- Name Name --- MType Morphological type ---- 4*E(B-V) Reddening mag UVmag FAUST UV magnitude mag e_UVmag rms uncertainty on FAUST UV magnitude mag l_GUV Limit flag on GUV --- GUV GUV UV magnitude (Kodaira et al., 1990ApJ...363..422K) number=1 All GUV measurements were transformed into monochromatic magnitudes. Note that each experiment measured at different spectral segment: GUV measured effectively at 1560{AA} with a bandwidth of FWHM=230{AA} SCAP measured at ~2000{AA} and the passband was ~200{AA}, and the Goddar imager (S+C) had a 1150{AA} wide passband centered near 2421{AA} mag e_GUV rms uncertainty on GUV mag SCAP SCAP UV magnitude (Donas et al., 1987A&A...180...12D) number=1 All GUV measurements were transformed into monochromatic magnitudes. Note that each experiment measured at different spectral segment: GUV measured effectively at 1560{AA} with a bandwidth of FWHM=230{AA} SCAP measured at ~2000{AA} and the passband was ~200{AA}, and the Goddar imager (S+C) had a 1150{AA} wide passband centered near 2421{AA} mag l_S+C Limit flag on S+C --- S+C S+C UV magnitude (Smith & Cornett, 1982, Cat. <VII/48>) number=1 All GUV measurements were transformed into monochromatic magnitudes. Note that each experiment measured at different spectral segment: GUV measured effectively at 1560{AA} with a bandwidth of FWHM=230{AA} SCAP measured at ~2000{AA} and the passband was ~200{AA}, and the Goddar imager (S+C) had a 1150{AA} wide passband centered near 2421{AA} mag Galaxies toward the Virgo cluster-multispectral data Source Source number --- Name Name --- TType T Type number=1 The T type is the translation of the morphological type(s) given in table 4, using the prescription from Table A of Tully 1988 (Cat. <VII/145>). --- UVmag FAUST UV magnitude mag e_UVmag rms uncertainty on UVmag mag l_FI(HI) Limit flag on FI(HI) --- FI(HI) H I flux integral (from the sources given in section 4.2) Jy.km/s FI(HI)2 Second value of FI(HI) for N=171 Jy.km/s S60um FIR flux densities at 60{mu}m number=2 From IRAS Faint Source Catalogue (Cat. <II/156>) Jy S100um FIR flux densities at 100{mu}m number=2 From IRAS Faint Source Catalogue (Cat. <II/156>) Jy HRV Heliocentric radial velocity number=3 Data originate from BST (Binggelli et al., 1985AJ.....90.1681B), RC3 (Cat. <VII/155>, or UGC (Cat. <VII/26>). km/s Btot Total B magnitude (3) number=4 Btot has been corrected for Galactic extinction, as explained in the text. mag --- --- Btot+ Additional Btot for sources 126 and 171 mag James Marcout, Patricia Bauer CDS 1997 Oct 13 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_111_143.xml An Einstein X-ray survey of optically selected galaxies. I. Data J/ApJS/111/163 J/ApJS/111/163 Einstein X-ray survey of galaxies. I. An Einstein X-ray survey of optically selected galaxies. I. Data D Burstein C Jones W Forman A P Marston R O Marzke Astrophys. J. Suppl. Ser. 111 163 1997 1997ApJS..111..163B IX/13 : The 2E Catalogue (Harris+ 1994) IX/15 : Einstein EMSS Survey (Gioia+ 1990, Stocke+ 1991) IX/18 : EINSTEIN extended source survey (EXSS) (Oppenheimer+ 1997) VII/112 : RC2 Catalogue (de Vaucouleurs+ 1976) VII/26 : Uppsala General Catalogue of Galaxies (UGC) (Nilson 1973) VII/115 : The surface photometry catalogue of the ESO-Uppsala galaxies Galaxies, optical Magnitudes X-ray sources catalogs galaxies: distances and redshifts surveys X-rays: galaxies The Einstein X-Ray Survey data consist of 3 separate kinds of files for each of our three data subsets: Tables 5-7: These tables give the basic observed data for the galaxies for which the authors were able to obtain X-ray data, both detections and upper limits. Included are both observed X-ray data and correlated optical data. Tables 9-11: These tables list the galaxies that were included in the search of the IPC images, but for which X-ray fluxes were not measured. A code explains why no measurement was made. Tables 12-14: These tables list the distance-dependent parameters, including predicted distance, method of predicted distance, X-ray luminosities or upper limits, absolute B optical diameters and absolute B magnitudes. We present the results of a complete Einstein imaging proportional counter X-ray survey of optically-selected galaxies from the Shapley-Ames Catalog (Cat. <VII/112>), the Uppsala General Catalog (Cat. <VII/26>) and the European Southern Observatory Catalog (Cat. <VII/115>). Well-defined optical criteria are used to select the galaxies, and X-ray fluxes are measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of <=0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F).The data presented here will be used in further studies to characterize the X-ray output of galaxies of various morphological types and thus to enable the determination of the major sources contributing to the X-ray emission from galaxies.
Einstein
Properties of Shapley-Ames galaxies with X-ray observations Name Name given in the RC2 (Cat. <VII/112>) Name for Shapley-Ames Galaxy given in RC2 (de Vaucouleurs et al., 1976, Cat. <VII/112> --- BT B mag as given in the RC2 Either BT (if given) or otherwise m_B_ as given in computer version of RC2. mag logD log of diameter in B band log of RC2 observed B mag diameter, log D_25, as observed, [0.1arcmin] MType Morphological type code, RC2 RC2 numerical code for galaxy morphological type, with the Burstein revision that I0 = -7 (not 0 as in RC2). --- IPCfield IPC Field Number (-1 if more than one) IPC Field Number on which X-ray flux was measured. If more than one IPC field was measured, a -1 is entered here, and the fields used are given in Table 8 of the paper. --- ExpTime Total exposure time for IPC field(s) Total exposure time for IPC images, summed over all observed fields. s RAh Right Ascension (1950), RC2 h RAm Right Ascension (1950), RC2 min DE- Declination sign --- DEd Declination (1950), RC2 deg DEm Declination (1950), RC2 arcmin CTXray X-ray count-rate X-ray count rate and error, in units of 1000 times observed count rate, only deadtime-corrected and background-corrected. ct/ks e_CTXray X-ray count-rate, 1-sigma error Error in X-ray count rate, taking into account all sources of random error. ct/ks Corr Correction factor to X-ray ct rate Multiplicative correction factor for HI column density and source energy 8 distribution, to transform vignetting-corrected and dead-time corrected source counts to X-ray flux in units of 10^{-11} ergs/cm2/s. --- Vignette Vignetting correction to X-ray count rate Vignetting correction, to be divided into observed count rate. --- ApCode Code for X-ray aperture size Numerical code for the largest aperture used to obtain the X-ray count rate. 1 = 200" aperture, 2 = 232" aperture, 3 = 264" aperture and 4 = 296" aperture. --- Properties of UGC galaxies with X-ray observations Name UGC (Cat. <VII/26>) number of galaxy --- Bmag B mag as given in the UGC (Cat. <VII/26>) If Bmag<=15.7, comes from Zwicky (1961-1968, Cat. <VII/49>) via Huchra (1976AJ.....81..952H) corrections. Otherwise it is just a rough estimate (accuracy 0.5-1.0 mag) by Nilson (1973, Cat. <VII/26>). mag logD log B diameter, UGC (Cat. <VII/26>) log of UGC Bmag diameter [0.1arcmin] MType Burstein morphological type code, UGC Burstein developed a hierarchical numerical typing system for Morphological types. The abbreviated system for the UGC and ESO catalogs is as follows: Burstein Code Number Classification 1 E and E/S0 10 All S0 11 All S0/a 12 All Sa 13 All Sa/b 14 All Sb 15 All Sb/Sc 16 All Sc 17 All Sc/Sd 18 All Sd 19 All Sd/Irr 20 All Irr 30 All non-divided classified types 40 Dwarf galaxies 50 Compact galaxies and N galaxies 60 Multiple systems 70 Peculiar galaxies 90 No galaxy class given --- IPCfield IPC Field Number (-1 if more than one) --- ExpTime Total exposure time for IPC field(s) s RAh Right Ascension 1950 Right Ascension and Declination are as determined either by Dressel & Condon (1976ApJS...31..187D) or by our own measurements. Accuracy of +/-8" in positions. h RAm Right Ascension 1950 min DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin CTXray X-ray count-rate ct/ks e_CTXray X-ray count-rate, 1-sigma error ct/ks Corr Correction factor to X-ray ct rate --- Vignette Vignetting correction to X-ray ct rate --- ApCode Code for X-ray aperture size --- Properties of ESO galaxies with X-ray observations Name ESO (Cat. <VII/115>) name for galaxy --- Bmag B mag, ESO-LV catalog B mag as given in the ESO-LV catalog (Lauberts & Valentijn, 1989, Cat. <VII/115>). 0.00 if no mag given. mag logD =-1.10 log of diameter in B band, ESO-LV log of ESO-LV B mag diameter at 25th mag isophote; -1.10 if no diameter given. [0.1arcmin] MType Burstein morphological type code, ESO-LV See the note for MType in table6.dat. --- IPCfiled IPC Field Number (-1 if more than one) --- ExpTime Total exposure time for IPC field(s) s RAh Right Ascension (1950), ESO-LV h RAm Right Ascension (1950), ESO-LV min DE- Declination sign --- DEd Declination (1950), ESO-LV deg DEm Declination (1950), ESO-LV arcmin CRXray X-ray count-rate ct/ks e_CRXray X-ray count-rate, 1-sigma error ct/ks Corr Correction factor to X-ray ct rate --- Vignette Vignetting correction to X-ray ct rate --- Ap_code Code for X-ray aperture size --- Shapley-Ames galaxies without X-ray observations UGC galaxies without X-ray observations ESO galaxies without X-ray observations Name Name (RC2, UGC or ESO) In table9.dat : Name for Shapley-Ames Galaxy given in RC2 (de Vaucouleurs et al. 1976, Cat. <VII/112>) In table10.dat: UGC (Cat. <VII/26>) number of galaxy In table11.dat: ESO (Cat. <VII/115>) name for galaxy --- BT B mag as given in the RC2, UGC or ESO-LV In table9.dat : Either B_T (if given) or otherwise Bmag as given in computer version of RC2 (Cat. <VII/112>) In table10.dat: Bmag as given in UGC ((Cat. <VII/26>). If B_T<=15.7, comes from Zwicky (1961-1968, Cat. <VII/49>); otherwise just a rough estimate (accuracy 0.5-1.0 mag). In table11.dat: B mag as given in the ESO-LV catalog (Lauberts & Valentijn 1989, Cat. <VII/115>). 0.00 if no mag given. mag exCode Reason for omission from survey Reason for omitting galaxy from X-ray survey: 0 = image not available in processed form; 2 = on IPC 'ribs'; 3 = on or off edge of IPC field; 4 = in obvious diffuse emission; 7 = too large for this survey 9 = only HRI image available. --- Derived properties of X-ray observed Shapley-Ames galaxies Derived properties of X-ray observed UGC galaxies Derived properties of X-ray observed ESO galaxies Name Name given in the RC2, UGC or ESO-LV In table12.dat: Name for Shapley-Ames galaxy as given in the RC2 (Cat. <VII/112>). In table13.dat: UGC (Cat. <VII/26>) number of galaxy In table14.dat: ESO (Cat. <VII/115>) name for galaxy --- HRV Heliocentric radial velocity The heliocentric velocity, from sources as cited in the paper, including: RC2 (Cat. <VII/112>), RC3 (Cat. <VII/155>), NASA Extragalactic Database (NED) km/s Dist Distance Distance based on the source of distance (r_Dist), assuming H_0_=75km/s/Mpc. Mpc r_Dist Source of distance A numerical code for the source of distance estimate. All independent distance measurements come from Willick et al. (1996ApJ...457..460W and ADC-distributed data base); see references therein for details of individual data sets. The abbreviations correspond to the notation of Willick et al. 1 = Faber et al. (1989, Cat. <VII/176>) 2 = Tormen & Burstein reanalysis of Aaronson et al. (1982, Cat. < VII/75>) H_-0.05_ magnitudes (A82); 3 = Han, Mould et al. Northern survey data (e.g., Han & Mould, 1992ApJ...396..453H; HM); 4 = Han, Mould et al. Southern survey data (e.g., Han & Mould, 1992ApJ...396..453H; HM); 5 = Courteau and Faber data (CF; Courteau, 1992, Ph.D. Thesis); 6 = Mathewson, Ford & Buchhorn (1992ApJS...81..413M; MAT); 7,8 = Willick (Willick et al., 1996ApJS..109..333W); 9 = from Faber-Burstein Great Attractor velocity field model for an associated cluster or a Local Group galaxy; 10 = from Faber-Burstein Great Attractor velocity field model for this galaxy; 90 = from Mark II data set (Burstein, 1989, Mark II Catalog of Galaxies Peculiar Velocities, email distribution); 99 = from Willick et al. (1996ApJS..109..333W) but observed 2 or more times. --- BMag Absolute blue magnitude In table12.dat: Absolute Blue mag, corrected for Galactic extinction from Burstein & Heiles (1984ApJS...54...33B and from the BH reddening maps) and redshift/K-corr via RC2 principles. For spiral and irregular galaxies, also corrected for inclination via the general RC3 relation: {delta}B_T=-1.5log(a/b), where a/b is the observed axial ratio. In table13.dat: 0.00 if no magnitude given In table14.dat: 0.00 if no magnitude given observed axial ratio. mag logDabs log of metric diameter In table12.dat: Absolute B mag diameter, 25th mag isophote, in kpc. Corrected for Galactic extinction only; no inclination correction made. In table14.dat: 0.00 if no distance given [kpc] l_logLXray Symbol if detected or upper limit Upper limit symbol. '<' if upper limit; >2.5{sigma} detection if blank. --- logLXray log of Absolute X-ray luminosity/upp-limit log of absolute X-ray luminosity, fully-corrected as described in the paper. [10-7W] SyCode Code if Seyfert galaxy A code for the type of Seyfert galaxy: blank = not a Seyfert 1 = Seyfert 1 2 = Seyfert 2 3 = Seyfert ? Seyfert classifications taken from NED. --- CDS 1998 Feb 06 AAS CD-ROM series, Volume 9, 1997, Lee Brotzman [ADS] 17-Jun-97 J_ApJS_111_163.xml A New Chemo-evolutionary Population Synthesis Model for Early-Type Galaxies. II. Observations and Results J/ApJS/111/203 J/ApJS/111/203 Chemo-evolutionary Population Synthesis II. A New Chemo-evolutionary Population Synthesis Model for Early-Type Galaxies. II. Observations and Results A Vazdekis R Peletier J E Beckman E Casuso Astrophys. J. Suppl. Ser. 111 203 1997 1997ApJS..111..203V Abundances Models, evolutionary galaxies: abundances galaxies: evolution galaxies: nuclei galaxies: stellar content We present the results of applying a new chemo-evolutionary stellar population model, developed in a previous paper, to new high-quality observational data of the nuclear regions of two representative elliptical galaxies and the bulge of the Sombrero galaxy. Here we fit in detail ~20 absorption lines and six optical and near-infrared colors, following two approaches: fitting a single-age, single-metallicity model and fitting our full chemical evolutionary model. We find that all the iron lines are weaker than the best-fitting models predict, indicating that the iron abundance is anomalous and deficient. We also find that the Ca I index at 4227 A is much lower than predicted by the models. We can obtain good fits for all the other lines and observed colors with models of old and metal-rich stellar populations and can show that the observed radial gradients are due to metallicity decreasing outward. We find that good fits are obtained both with fully evolutionary models and with single-age, single-metallicity models. This is due to the fact that in the evolutionary model more than 80% of the stars form within 1.5 Gyr after the formation of the galaxies. The fact that slightly better fits are obtained with evolutionary models indicates that these galaxies contain a small spread in metallicity.
NGC 3379 10 47.8 +12 35 NGC 4472 12 29.7 +07 59 NGC 4594 12 40.0 -11 37
Absorption indices vs. radius for NGC 3379 Absorption indices vs. radius for NGC 4472 Absorption indices vs. radius for NGC 4594 Line Line identification --- Dist Distance to the galactic center at each side of the center arcsec Index Index value Index value in {AA} except for the CN1, CN2, Mg1, Mg2 and TiO1 bands which are given in 'magnitudes' --- e_Index Estimated error in Index --- Patricia Bauer CDS 1997 Jul 09 AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 29-Apr-97 J_ApJS_111_203.xml H{gamma} and H{delta} absorption features in stars and stellar populations J/ApJS/111/377 J/ApJS/111/377 H{gamma} & H{delta} absorption features H{gamma} and H{delta} absorption features in stars and stellar populations G Worthey D L Ottaviani Astrophys. J. Suppl. Ser. 111 377 1997 1997ApJS..111..377W Balmer lines Equivalent widths Populations, stellar galaxies: evolution galaxies: stellar content line: profiles stars: abundances The H{gamma} and H{delta} absorption features are measured in a sample of 455 (out of an original 460) Lick IDS stars with pseudo-equivalent width indices. For each Balmer feature, two definitions, involving a narrow (~20{AA}) and a wide (~40{AA}) central bandpass, were measured. These four new Balmer indices augment 21 indices previously determined by Worthey et al., and polynomial fitting functions that give index strengths as a function of stellar temperature, gravity, and [Fe/H] are provided. The new indices are folded into models for the integrated light of stellar populations, and predictions are given for single-burst stellar populations of a variety of ages and metallicities. Contrary to our initial hopes, the indices cannot break a degeneracy between burst age and burst strength in poststarbust objects, but they are successful mean-age indicators when used with sensitive metallicity indicators. An appendix gives data, advice, and examples of how to transform new spectra to the 25-index Lick IDS system.
Index measurements HD Henry Draper (Cat. <III/135>) number --- m_HD Multiplicity index on HD --- Other1 First alternate star name --- Other2 Second alternate name --- HdeltaA Index equivalent width The "A" means that the wider (~40{AA}) definition measures most of the absorption present in A stars, and the narrower (~20{AA}) "F" definition catches most of the absorption of an F star but very little of the very wide profile of an A star. Spectra for HR 296, HR 1726, HR 2047, HR 2503, and HR 2506 were lost subsequent to Faber et al. (1985ApJS...57..711F), and do not appear in this table. Most other missing data are due to the spectrograph settings in some runs that excluded the bluest parts of the spectrum. Other data were deleted if irregularities were present in the spectra. 0.1nm HgammaA Index equivalent width 0.1nm HdeltaF Index Equivalent width 0.1nm HgammaF Index equivalent width 0.1nm NdA Number of H{delta}A measurements --- NgA Number of H{gamma}A measurements --- NdF Number of H{delta}F measurements --- NgF Number of H{gamma}F measurements --- Qual Quality The quality parameter is normally one, but is 2 if the errors are judged about twice as large as the value in Table 1 of the printed paper, and 3 if the errors are judged three times the Table 1 value or larger. --- CDS 1998 Feb 06 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 25-Jul-97 J_ApJS_111_377.xml Medium resolution spectra of normal stars in the K band J/ApJS/111/445 J/ApJS/111/445 Spectra of normal stars in the K band Medium resolution spectra of normal stars in the K band L Wallace K Hinkle Astrophys. J. Suppl. Ser. 111 445 1997 1997ApJS..111..445W Atlases Spectra, infrared Stars, normal atlases infrared: stars stars: carbon stars: early-type stars: late-type stars: variables: other (Mira) An Atlas of 115 medium-resolution K-band (2.0-2.4um) stellar spectra, spanning spectral types O-M and luminosity types I-V, is presented. K-band spectra are also presented for one N- and one J-type carbon star. A time series of spectra is presented for an S-type Mira variable. All the spectra are at a resolution of ~3000 (1.4cm^-1^) and have had the terrestrial absorption removed by dividing a featureless spectrum. The spectra are plotted with the major spectral features identified and are available digitally.
List of objects observed File File name of spectrum in subdirectory sp --- Name Star name --- Other Alternate star name --- Sp Spectral type --- Notes Notes, date & FTS scan nos., ref. star, and other details such as water vapor correction --- Spectral data Freq Frequency scale The frequency scale where all stars have been interpolated onto a scale from 4150.0 to 4950.0cm^-1^ at intervals of 0.5cm^-1^. cm-1 FiltSum Filtered sum The fully processed version of the spectrum described in section 3 of the printed paper. --- FiltDiff Filtered difference The fully processed difference of the forward and backward scans, which gives an objective measure of the S/N in the processed spectrum. --- UnfiltSum Unfiltered sum A version of the spectrum which is processed but not filtered. Specifically, the notch filter designed to remove the 3.4cm^-1^/cycle ringing and the apodizing filter were not applied. This version is included because for some purposes less filtering can clarify some questions. --- n_UnfiltSum Note (NaN) --- CDS 1998 Feb 06 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 25-Jun-97 J_ApJS_111_445.xml A Near-Infrared Imaging Survey of the Rho Ophiuchi Cloud Core J/ApJS/112/109 J/ApJS/112/109 Rho Oph Near IR Positions and Photometry A Near-Infrared Imaging Survey of the Rho Ophiuchi Cloud Core M Barsony S J Kenyon E A Lada P J Teuben Astrophys. J. Suppl. Ser. 112 109 1997 1997ApJS..112..109B Associations, stellar Infrared sources Interstellar medium - Photometry, infrared Positional data Selected areas This catalog contains the tabulated results from a three-color (JHK) near-Infrared imaging survey of the Rho Ophiuchi star-forming cloud core. The NIR imaging observations were acquired using the SQIID instrument on the Kitt Peak 1.3m telescope from June 4-10, 1993 and April 23-28, 1994. The survey covered one square degree (2.2pc by 2.2pc). The catalog contains 4495 sources with both J2000.0 and B1950.0 coordinates for each source and its J, H, and K magnitudes and/or upper their limits. The Rho Ophiuchi clouds are of great interest for star formation studies, since they include the nearest example of a currently forming star cluster. The absolute positions in RA and Dec were determined for each individual source by using a centering algorithm in the IRAF package APPHOT to obtain center positions in pixels which were then merged into a single common positional grid. Absolute stellar coordinates were determined by comparing the authors positional database with the positions of 36 HST Guide Star Catalog stars spread out over the survey field. These were used to determine a plate scale and rotation which was used to generate the final list of source positions. The position determination technique and the photometric data reduction and calibration is discussed in detail in the source reference.
Previous rho Oph near-infrared surveys Survey Survey designation (shortened) --- Sources Number of sources --- Res Spatial resolution arcsec Area Area covered by survey (square arcminutes) arcmin2 n_Area Note on Area (c) The 119 sources SKS detected refer only to sources which are confined to the rho Oph A, rho Oph B, and rho Oph E/F cloud cores, comprising less than half of their entire survey area. (d) WLY conducted an IRAS-selected survey in the K band. They examined 42 fields of 1 square arcmin toward 26 IRAS sources. --- limitK Limiting K magnitude of survey mag colors Photometric bands covered --- n_colors Note on colors (a) VSSG published J photometry for 11 sources, H photometry for 28 sources, and L photometry for four sources of their list and JHKL photometry of eight sources from the list of GSS. (b) Elias chose 50 sources with H-K > 0.7 for follow-up photometry at bands other than K. --- ref Survey reference --- Rho Oph NIR source positions and JHK photometry BKLT_J Source BKLT J designation --- Comp Source component --- RAh Right Ascension hours (J2000.0) h RAm Right Ascension minutes (J2000.0) min RAs Right Ascension seconds (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination degrees (J2000.0) deg DEm Declination minutes (J2000.0) arcmin DEs Declination seconds (J2000.0) arcsec RA1950h Right Ascension hours (B1950.0) h RA1950m Right Ascension minutes (B1950.0) min RA1950s Right Ascension seconds (B1950.0) s DE1950- Declination sign (B1950.0) --- DE1950d Declination degrees (B1950.0) deg DE1950m Declination minutes (B1950.0) arcmin DE1950s Declination seconds B1950.0) arcsec l_Jmag Limit flag on J magnitude --- Jmag J magnitude mag l_Hmag Limit flag on H magnitude --- Hmag H magnitude mag l_Kmag Limit flag on k magnitude --- Kmag K magnitude mag Near-infrared cross identifications BKLT_J Source BKLT J designation --- Comp Source component --- l_Jmag Limit flag on J magnitude --- Jmag J magnitude mag l_Hmag Limit flag on H magnitude --- Hmag H magnitude mag l_Kmag Limit flag on k magnitude --- Kmag K magnitude mag GY GY source identification --- n_GY Notes on GY See notes described in file "tab3note.txt". --- WL WL source identification --- n_WL Notes on WL --- VSSG VSSG source identification --- n_VSSG Notes on VSSG --- GSS GSS source identification --- n_GSS Notes on GSS --- Elias Elias source identification --- n_Elias Notes on Elias --- BBRCG BBRCG source identification --- n_BBRCG Notes on BBRCG --- CRBR BBRCG source identification --- n_CRBR Notes on CRBR --- SKS SKS source identification --- n_SKS Notes on SKS --- WLY WLY source identification --- n_WLY Notes on WLY --- Photometry Comparisons between surveys Survey Survey name(s) --- Ntot Total number of sources detected --- Nrec Number of sources recovered --- N(K) Number of K measurements used in fit --- N(H) Number of H measurements used in fit --- N(J) Number of J measurements used in fit --- A(K) Intercept of K band linear fit mag sigmaA(K) One sigma error of A(K) mag B(K) Slope of K band linear fit --- sigmaB(K) One sigma error of B(K) --- a(K) Absolute deviation about the K band fit --- A(H) Intercept of H band linear fit mag sigmaA(H) One sigma error of A(H) mag B(H) Slope of H band linear fit --- sigmaB(H) One sigma error of B(H) --- a(H) Absolute deviation about the H band fit --- A(J) Intercept of J band linear fit mag sigmaA(J) One sigma error of A(J) mag B(J) Slope of J band linear fit --- sigmaB(J) One sigma error of B(J) --- a(J) Absolute deviation about the J band fit --- Variable Sources BKLT_J Source BKLT J designation --- mean(K) Mean K magnitude mag sigma(K) Standard deviation of K measurements mag mean(H) Mean H magnitude mag sigma(H) Standard deviation of H measurements mag mean(J) Mean J magnitude mag sigma(J) Standard deviation of J measurements mag N(K) Number of K band measurements --- tab3note.txt Notes for table3.dat James E. Gass ADC/SSDOO 1998 Apr 08 UNKNOWN UNKNOWN The file table2.dat contains corrections to the declinations as provided by the authors. J_ApJS_112_109.xml Search and redshift survey for IRAS galaxies behind the Milky Way and structure of the Local Void J/ApJS/112/245 J/ApJS/112/245 Redshift survey for IRAS galaxies Search and redshift survey for IRAS galaxies behind the Milky Way and structure of the Local Void K Nakanishi T Takata T Yamada T T Takeuchi R Shiroya M Miyazawa S Watanabe M Saito Astrophys. J. Suppl. Ser. 112 245 1997 1997ApJS..112..245N VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991) VII/209 : Catalog of Gal. Behind the Milky Way (Saito+ 1990-91, Roman+ 1996-98) II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) J/A+AS/104/529 : IRAS galaxies behind the Milky Way (Takata+ 1994) Galaxies, IR Redshifts catalogs infrared: galaxies large-scale structure of universe surveys This is the third and final paper (Yamada et al., 1993ApJS...89...57Y and Takata et al., Cat. <J/A+AS/104/529>) of our systematic visual search for IRAS galaxies behind the Milky Way at |b|<=15{deg}. This paper presents a catalog of 950 IRAS galaxies with 60{mu}m flux densities larger than 0.6Jy located between l=0{deg} and 150{deg}, of which 293 are newly identified by this search. We made a redshift survey for the identified galaxies and obtained new redshift data of 171 galaxies. We also present newly measured redshifts of 27 IRAS galaxies between l=150{deg} and 225{deg} at |b|<=15{deg}. In this paper we studied the structure of the Local void using IRAS galaxies and galaxies from the Third Reference Catalogue of Bright Galaxies (Cat. <VII/155>) in the region l=30{deg}-120{deg} and b=-50{deg} to +30{deg}. The center of the Local void turned out to be located at l~60{deg}, b~-15{deg}, and cz~2500km/s, and the size is about 2500km/s along the direction toward the center.
The catalog of IRAS galaxies with F60>=0.6Jy IRAS IRAS (Cat. <II/125>) point source name --- m_IRAS Multiplicity index in IRAS --- GLON Galactic longitude deg GLAT Galactic latitude deg F60um Flux density at 60{mu}m Jy F100um Flux density at 100{mu}m Jy Gal? G: galaxy; G?: possible galaxy --- MType Morphological type number=1 E: elliptical galaxy S: spiral galaxy I: Irregular galaxy E/S: galaxy we could not classified --- Dmaj Major axis diameter (1mm = 67") mm Dmin Minor axis diameter (1mm = 67") mm Note Emulsion number=2 I: UK Schmidt I film copy J: ESO/SRC J film copy blank: POSS E paper prints --- Com Comment on multiplicity number=3 For multiplicity: pair: two galaxies are located within a separation as wide as the galaxy sizes tri: triplet group: group of galaxies int: two galaxies appear to be interacting For image appearance: PN?: possible planetary nebula LSB: low surface brightness HSB: high surface brightness ND: nuclear dominated pec: peculiar. --- cz Heliocentric radial velocity km/s r_cz Reference for cz number=4 A: Measurement at OAO by us 1: RC3, de Vaucouleurs et al. (1991, Cat. <VII/155>) 2: General Catalog of H I Observations of Galaxies (Huchtmeier & Richter, 1989, New York: Springer) 3: "1.936 Jy sample" by Strauss et al. (1992, Cat. <II/174>) 4: Lu et al. (1990ApJ...357..388L) 5: Seeberger, Huchtmeier, & Weinberger (1994, Cat. <J/A+A/286/17>) 6: Bottinelli et al. (1994, ASP Conf. Ser. 67, 225) 7: "1.2 Jy sample" by Fisher et al. (1995, Cat. <VII/185>) 8: Kraan-Korteweg et al. (1994Natur.372...77K) 9: Weinberger, Saurer & Seeberger (1995, Cat. <J/A+AS/110/269>) 10: Marzke, Huchra, & Geller (1996, Cat. <J/AJ/112/1803>) 11: The IRAS PSC Redshift Survey (PSCz)" and the extension to low latitude BTP survey by Saunders et al. (1997, Priv. Comm.) --- Ident Cross-identification --- Radial velocities of IRAS galaxies with F60>=0.6Jy at 150<l<225 and |b|<=15 IRAS IRAS point source name --- GLON Galactic longitude deg GLAT Galactic latitude deg F60um Flux density at 60{mu}m Jy F100um Flux density at 100{mu}m Jy cz Heliocentric radial velocity (this paper) km/s Ident Cross-identification --- James Marcout, Patricia Bauer CDS 1998 Apr 03 UNKNOWN UNKNOWN From the ApJS electronic version J_ApJS_112_245.xml Properties that cannot be explained by the progenitors of planetary nebulae J/ApJS/112/487 J/ApJS/112/487 Planetary nebulae classification Properties that cannot be explained by the progenitors of planetary nebulae N Soker Astrophys. J. Suppl. Ser. 112 487 1997 1997ApJS..112..487S V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) Planetary nebulae catalogs ISM: structure planetary nebulae: general stars: evolution I classify a large number of planetary nebulae (458) according to the process that caused their progenitors to blow axisymmetrical winds. The classification is based primarily on the morphologies of the different planetary nebulae, assuming that binary companions, stellar or substellar, are necessary in order to have axisymmetrical mass loss on the asymptotic giant branch. I propose four evolutionary classes, according to the binary-model hypothesis: (1) Progenitors of planetary nebulae that did not interact with any companion. These amount to ~10% of all planetary nebulae. (2) Progenitors that interact with stellar companions that avoided a common envelope, 11^+2^_-3_% of all nebulae. (3) Progenitors that interact with stellar companions via a common envelope phase, 23^+11^_-5_% of all nebulae. (4) Progenitors that interact with substellar (i.e., planets and brown dwarfs) companions via a common envelope phase, 56^+5^_-8_% of all nebulae. In order to define and build the different classes, I start with clarifying some relevant terms and processes related to binary evolution. I then discuss kinematical and morphological properties of planetary nebulae that appear to require the interaction of the planetary nebula progenitors and/or their winds with companions, stellar or substellar.
Single-progenitor PNe A close stellar companion which avoided common envelope Common envelope with a stellar companion Common envelope with a substellar companion </tableLink> </tableLinks> <fields> <field> <name>Object</name> <definition>Object name</definition> <units>---</units> </field> <field> <name>PNG</name> <definition>PN G designation as in Catalog <V/84></definition> <units>---</units> </field> <field> <name>Conf</name> <definition>Confidence <footnote footnoteId="???"> <para>number=1</para> <para>In table2 and table4, L means that the PNe may belong to table5 LL means that it may belong to table 3 In table3 and table5, L means that the PNe may belong to table4</para> </footnote> </definition> <units>---</units> </field> <field> <name>Dev</name> <definition>Deviation <footnote footnoteId="???"> <para>number=2</para> <para>The letters in parentheses following the ISM mark give the direction of the PN relative to the ISM. WB: the deviation from axisymmetry is caused by a wide binary ISM/WB: the deviation may be caused by the ISM or a wide binary EWB: possible presence of an extreme-wide-binary ISM-B: possibility that the ISM-magnetic field shaped the structure on the outskirts Question mark following ISM means that it is hard to tell from the image whether the ISM really influences the PN morphology.</para> </footnote> </definition> <units>---</units> </field> <field> <name>Com</name> <definition>Comments <footnote footnoteId="???"> <para>number=3</para> <para>PO stands for `pole-on', which means that these PN may be ellipticals observed pole-on. CB signifies PNe which are known to have close binary central stars (Bond 1995, Ann. Israel Phys. Soc. 11, 61) (No PN G): PNe which are not listed in the catalogue of Acker et al. (1992, Cat. <V/84>)</para> </footnote> </definition> <units>---</units> </field> </fields> </tableHead> <textFile xlink:href="tables.tex"> <name>tables.tex</name> <description> <para>LaTeX version of the tables</para> </description> </textFile> <history> <ingest> <creator> <lastName>Patricia Bauer</lastName> <affiliation>CDS</affiliation> </creator> <date> <year>1997</year> <month>Dec</month> <day>12</day> </date> <acknowledgement>Soker Noam <soker@physics.technion.ac.il></acknowledgement> </ingest> </history> <identifier>J_ApJS_112_487.xml</identifier> </dataset> <dataset subject="astronomy" xmlns:xlink="http://www.w3.org/XML/XLink/0.9"> <title>Classification and Identification of IRAS Sources With Low-Resolution Spectra J/ApJS/112/557 J/ApJS/112/557 Classification of IRAS Sources Classification and Identification of IRAS Sources With Low-Resolution Spectra S Kwok K Polk W P Bidelman Astrophys. J. Suppl. Ser. 112 557 1997 1997ApJS..112..557K III/197 : IRAS Low Resolution Spectra (IRAS team, 1987) Bidelman, W.P, =1987IAUS..122..217B Hoffleit D., =1982bsc..book....H (Catalog: V/25B) Kholopov P.N. et al., =1992BICDS..40...15K (Catalog: II/139B) Kukarkin B.V. et al., =1982ncsv.book.....K (Catalog: II/140) Neugebauer, G. & Leighton, R. B., =1969tmss.book.....N (Catalog: II/2B) Price, S.D. & Murdock, T.L., =1983AFGL..161.....P (Catalog: II/94) Stephenson C.B., =1989PW&SO...3...53S (Catalog: III/156) Stephenson C.B., =1984gcss.book.....S (Catalog: III/168) Sweeney L.H. et al. 1978, Interim Equatorial Infrared Catalog, TR-0078-(3409-20)-1, Aerospace Corp. Cross identifications Infrared sources Interstellar medium Spectral types catalogs circumstellar matter infrared: stars stars: AGB and post-AGB stars: fundamental parameters IRAS low-resolution spectra were extracted for 11,224 IRAS sources. These spectra were classified into astrophysical classes, based on the presence of emission and absorption features and on the shape of the continuum. Counterparts of these IRAS sources in existing optical and infrared catalogs are identified, and their optical spectral types are listed if they are known. The correlations between the photospheric/ optical and circumstellar/infrared classifications are discussed.
IRAS
IDs, classes, 12 micron fluxes, 12-25 um colors IRAS IRAS Source name The IRAS sources in order of increasing right ascension (J1950) with the PSC designation. --- SAO SAO designation The probable SAO catalog number of the source, taken mainly but not entirely from the PSC. Because of the SAO catalog's accurate positions, identifications with its stars are considerably more secure than those with less accurate coordinates. --- HD_BD HD or BD designation Probable identifications with Henry Draper stars, or, for objects not included therein, with stars listed in the Bonner or Cordoba Durchmusterungs. Henry Draper Extension numbers are not used. The use of the Cordoba catalog for the entire southern sky seems appropriate for red stars that would perhaps not be contained in the Cape Photographic Durchmusterung (CPD); note that this is not the convention followed in the HD or SAO catalogs. A very few CPD designations have been used for stars not in the Cordoba Durchmusterung. The Durchmusterung designation originally contained an extended ASCII character for the degree symbol, (0xf8, decimal 248). This has been replaced with a blank to separate the declination from the number (e.g. +26 4746). --- GCVS GCVS designation Variable star name from the General Catalogue of Variable Stars (GCVS; Kholopov et al. 1985-1987), or in the New Catalogue of Variable Stars (NSV; Kukarkin et al. 1982). --- IRC IRC designation Identification from the CalTech Two-Micron Survey (Neugebauer & Leighton 1969; see Cat. <II/2>). --- AFGL AFGL designation Identification from the Revised AFGL Infrared Sky Survey Catalogue (Price & Murdock 1983; see Cat. <II/94>). --- Other Other designation Identification from the Bright Star Catalogue (Hoffleit 1982), with either their Bayer Greek letter or Flamsteed numbers or with their HR numbers. Identifications with carbon and S-type stars from Stephenson's (1984, 1989) comprehensive catalogs use "CS" or "SS", respectively. Also listed are the objects included in the First Interim Equatorial Catalog (EIC; Sweeney et al. 1978). Various other identifications are made with HII regions, planetary nebulae, emission-line objects contained in the Mount Wilson catalog and so on. --- Sp Optical spectral type Optical spectral types of the IRAS sources that are considered stellar, compiled from a number of disparate sources by W. P. Bidelman. The symbols in parenthesis are interpreted as follows: (PN) - the object is thought to be a planetary nebula (neb) - the source is believed to be a nebula (H II) - the source either has been detected as an H II region by radio continuum observations or is a well-known bright nebula (SiC) - the object has not been optically classified as a carbon star but the LRS spectrum shows the 11.3 um emission feature of SiC. --- LRS LRS classification --- Flux_12 12 um IRAS flux Jy C12-25 12um-25um color Jy Peak_12 12 um Peaker "25 um Peakers" (see Bidelman 1987, in IAU Symp. 122, Circumstellar Matter, ed. I. Appenzeller & C. Jordan (Dordrecht: Reidel), 217), IRAS sources whose flux density at 25 um is higher than their flux densities at 12 and 60 um. -------------------------------------------------------------------------------- History: * 27-Jul-1997: Prepared by Lee Brotzman for AAS CD-ROM series, Volume 9, 1997 * 29-Jan-1999: Standardized ReadMe by James E. Gass [SSDOO/ADC] * 27-Mar-1999: Corrections made at CDS by Fabienne Woelfel and Francois Ochsenbein on table1.dat (table1.tsv unchanged): GCVS names for sources IRAS 11472-0800, 12276-6435, 14281-6318, 17237-3011, 18320-1918, 18320-3502 ; PK (planetary nebulae) for sources IRAS 04395+3601, 09530-5704, 12171-6238, 17383-3004 (K 1-4 removed) IRAS number of RAFGL 4611S changed from 07316+2851 to 07316+2851 --- James E. Gass SSDOO/ADC 1999 Jan 29 AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 27-Jul-97 UNKNOWN UNKNOWN As submitted by the authors to the AAS CD-ROM Series, fields in table1.dat were separated by tabs. To meet the CDS/ADC standards, these have been translated at ADC into fixed-width fields. J_ApJS_112_557.xml Optically thick winds from degenerate dwarfs. I. Classical nova of populations I and II J/ApJS/113/121 J/ApJS/113/121 Optically thick winds from degenerate dwarfs. I. Optically thick winds from degenerate dwarfs. I. Classical nova of populations I and II M Kato Astrophys. J. Suppl. Ser. 113 121 1997 1997ApJS..113..121K Novae Models, evolutionary novae, cataclysmic variables stars: evolution stars: interior stars: mass-loss white dwarfs X-rays: stars Twenty-six sequences of optically thick wind solutions have been calculated which mimic the time-dependent evolution of classical novae of populations I and II. The peak of the new opacity around log T=5.2 due to iron lines is found to be strong enough to accelerate the winds even in very low iron abundance such as Z=0.001 for massive white dwarfs (>=0.8M_{sun}_). The old population novae show the slow light curve, the long X-ray turn-off time, the small expansion velocity and the small wind mass-loss rate. The X-ray turn-off time is a good indicator of the white dwarf mass because of its strong dependence on the white dwarf mass and weak dependence on the populations. The white dwarf mass is estimated to be ~0.6M_{sun}_ for GQ Mus and ~1.0M_{sun}_ for V1974 Cyg. The systematic difference of the wind velocity is predicted between novae in globular clusters and in galactic disk. Twenty-six tables are presented in the computer readable form of CD-ROM that consists of solutions of the optically thick wind and the static for the decay phase of classical novae with composition of X=0.35, C=0.1 and O=0.2 and heavy elements content Z=0.001, 0.004, 0.02, 0.05 and 0.1 for the white dwarf masses of 0.4, 0.6, 0.7, 0.8, 0.9, 1.0, 1.2 and 1.35M_{sun}_. These tables list the characteristic values of the envelope such as the photospheric temperature, the velocity, the wind mass-loss rate and fluxes of four wavelength bands. The updated OPAL opacity (Iglesias & Rogers, 1996ApJ...464..943I) is used.
Overall model parameters for all tables Table Table number (in the printed paper) --- Model Model name --- MassWD White dwarf mass solMass Z Heavy elements content --- RowWS Number of rows of (wind + static) solutions --- RowTot Number of rows total --- Envelope solutions for classical novae (table1 to table26) MassWD White dwarf mass solMass Z Heavy elements content --- log(Tph) Photospheric temperature [K] log(Lph) Photospheric luminosity [10-7W] log(Rph) Photospheric radius [solRad] log(Vph) Photospheric velocity [cm/s] log(Menv) Envelope mass [solMass] log(dM/dtw) Mass loss rate due to optically thick wind (log dM/dt (wind)) [solMass/yr] log(dM/dtn) Mass loss rate due to Hydrogen nuclear burning (log dM/dt (nuc)) [solMass/yr] Radcr Radius at the critical point solRad Velcr Velocity at the critical point cm/s time Evolutional time yr Mbol Bolometric magnitude mag Mvis Visual magnitude mag log(FUV) Flux in UV (912.3250{AA}) log(FNN) = log(L_NN_/4{pi}D^2^), D=1.0 kpc (NN=UV, EUV or SSXR) For log(FSSXR), values less than -30.000 are listed as just -30.000. [solLum/kpc2] log(FEUV) Flux in EUV (100.912{AA}) [solLum/kpc2] log(FSSXR) Flux in supersoft X-ray (30.100{AA}) [solLum/kpc2] UNKNOWN 1998 Feb 06 J_ApJS_113_121.xml Steps toward determination of the size and structure of the broad-line region in active galactic nuclei. XII. Ground-based monitoring of 3C 390.3. J/ApJS/115/185 J/ApJS/115/185 3C 390.3 BVRI and H photometry Steps toward determination of the size and structure of the broad-line region in active galactic nuclei. XII. Ground-based monitoring of 3C 390.3. M Dietrich B M Peterson P Albrecht M Altmann A J Barth P J Bennie R Bertram N G Bochkarev H Bock J M Braun A Burenkov S Collier L -Z Fang O P Francis A V Filippenko C B Foltz W Gaessler C M Gaskell M Geffert K K Ghosh R W Hilditch R K Honeycutt K Horne J P Huchra S Kaspi M Kuemmel K M Leighly D C Leonard Y F Malkov V Mikhailov H R Miller A C Morrill J Noble P T O'Brien T D Oswalt S P Pebley M Pfeiffer V I Pronik B -C Qian J W Robertson A Robinson K S Rumstay J Schmoll S G Sergeev E A Sergeeva A I Shapovalova D R Skillman S A Snedden S Soundararajaperumal G M Stirpe J Tao G W Turner R M Wagner S J Wagner J Y Wei H Wu W Zheng Z L Zou Astrophys. J. Suppl. Ser. 115 185 1998 1998ApJS..115..185D Active gal. nuclei Photometry, H-alpha Photometry, H-beta Photometry, H-gamma Photometry, UBVRI galaxies: active galaxies: individual (3C 390.3) galaxies: Seyfert Results of a ground-based optical monitoring campaign on 3C 390.3 in 1994-1995 are presented. The broadband fluxes (B, V, R, and I), the spectrophotometric optical continuum flux F_{lambda}_(5177{AA}), and the integrated emission-line fluxes of H{alpha}, H{beta}, H{gamma}, He I 5876, and He II {lambda}4686 all show a nearly monotonic increase with episodes of milder short-term variations superposed. The amplitude of the continuum variations increases with decreasing wavelength (4400-9000{AA}). The optical continuum variations follow the variations in the ultraviolet and X-ray with time delays, measured from the centroids of the cross-correlation functions, typically around 5 days, but with uncertainties also typically around 5 days; zero time delay between the high-energy and low-energy continuum variations cannot be ruled out. The strong optical emission lines H{alpha}, H{beta}, H{gamma}, and He I {lambda}5876 respond to the high-energy continuum variations with time delays typically about 20 days, with uncertainties of about 8 days. There is some evidence that He II {lambda}4686 responds somewhat more rapidly, with a time delay of around 10 days, but again, the uncertainties are quite large (~8 days). The mean and rms spectra of the H{alpha} and H{beta} line profiles provide indications for the existence of at least three distinct components located at +/-4000 and 0km/s relative to the line peak. The emission-line profile variations are largest near line center.
QSO 1845+796 3C 390.3 18 42 09.1 +79 46 17
H{alpha} blue light curve H{alpha} center light curve H{alpha} red light curve H{alpha} total light curve H{beta} blue light curve H{beta} center light curve H{beta} red light curve H{beta} total light curve He II 4686 light curve He I 5876 light curve H{gamma} light curve HJD Heliocentric Julian date d Flux Flux 10-15mW/m2 e_Flux rms uncertainty on Flux 10-15mW/m2 Continuum at 5177{AA} light curve B-band photometry light curve V-band photometry light curve R-band photometry light curve I-band photometry light curve HJD Heliocentric Julian date d Flux Flux 10-14W/m2/nm e_Flux rms uncertainty on Flux 10-14W/m2/nm James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN //www.astronomy.ohio-state.edu/~agnwatch/3c390/ J_ApJS_115_185.xml The MX northern Abell cluster redshift survey. J/ApJS/115/1 J/ApJS/115/1 MX northern Abell cluster redshift survey The MX northern Abell cluster redshift survey. K Slinglend D Batuski C Miller S Haase K Michaud J M Hill Astrophys. J. Suppl. Ser. 115 1 1998 1998ApJS..115....1S VII/110 : Rich Clusters of Galaxies (Abell+ 1989) Clusters, galaxy Redshifts galaxies: clusters: general galaxies: distances and redshifts large-scale structure of universe The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, & Olowin catalogs (Cat. <VII/110>) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R>=1 Abell cluster fields with m10 less than or equal to 16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.
MX survey cluster velocities Cluster Abell cluster name --- m_Cluster Multiplicity index on Cluster --- n_Cluster Note on Cluster number=1 * : Includes five galaxies from CfA survey. --- m10 Magnitude of the tenth brightest galaxy in the cluster mag Class Bautz-Morgan (1970ApJ...162L.149B) class --- mu Mean velocity km/s n_mu Note on {mu} velocity number=2 A: Clusters that not have enough measured galaxies for a clear determination C: Clusters that are not clusters at all but rather are simply many galaxies (i.e. 15 or so observed) along the line of sight. --- CBI Biweight estimate of the data's central location km/s sigma Standard deviation velocity km/s SBI Biweight estimate of the data's scale km/s Ncluster Number of galaxy velocities (within each group) that went into each calculation --- Note Notes number=3 *: Mean velocity is the accepted velocity b: Clearly identified background group f: Clearly identified foreground group --- Individual galaxy velocities Cluster Abell cluster name number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD --- RAh Right ascension (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD h RAm Right ascension (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD min RAs Right ascension (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD s DE- Declination sign number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD --- DEd Declination (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD deg DEm Declination (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD arcmin DEs Declination (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD arcsec Vel Velocity km/s n_Vel Note on Vel number=2 a : cD galaxy or brightest central galaxy in the cluster. --- e_Vel rms uncertainty on Vel km/s James Marcout, Patricia Bauer CDS 1998 Oct 16 UNKNOWN UNKNOWN //kramer.ume.maine.edu/~panda/phyast/mxdata J_ApJS_115_1.xml The Five College Radio Astronomy Observatory CO Survey of the Outer Galaxy J/ApJS/115/241 J/ApJS/115/241 The FCRAO CO Survey of the Outer Galaxy The Five College Radio Astronomy Observatory CO Survey of the Outer Galaxy M H Heyer C Brunt R L Snell J E Howe F P Schloerb J M Carpenter Astrophys. J. Suppl. Ser. 115 241 1998 1998ApJS..115..241H Carbon monoxide Interstellar matter Radio sources Surveys Galaxy: structure ISM: clouds ISM: general ISM: kinematics and dynamics ISM: molecules surveys The FCRAO CO survey of the Outer Galaxy is comprised of 1,696,800 12CO J=1-0 spectra sampled every 50 arcsec between Galactic longitudes 102.49 and 141.54 degrees, and latitudes -3.03 and 5.41 degrees. The spatial resolution (half-power beamwidth) of the survey is 45 arcsec. The V(LSR) ranges from -153 to +40 km/s sampled every 0.81 km/s with a velocity resolution of 0.98 km/s. The survey provides the highest spatial dynamic range imaging of the molecular interstellar medium obtained to date. For a discussion of survey sensitivity, systematics and image artifacts, see the journal article (1998 ApJS 115, 241). The 336 square-degree region of the survey encompasses 79 optical HII regions (Blitz, Fich & Stark 1982) and hundreds of IRAS point sources with colors characteristic of young stellar objects (Wouterloot & Brand 1989). The survey data are ideally suited to address 1) the topology of the molecular interstellar medium, 2) the relationship between the molecular and atomic gas in the interstellar medium, 3) the relationship of molecular regions to spiral arms, and 4) the size and mass distributions of molecular clouds. The survey data are archived as 606 files. Each file is in FITS image format, and maps the 12CO antenna temperature at a fixed Galactic latitude for the survey's (Galactic longitude, V(LSR)) sampling grid. File 001 starts at Galactic latitude -3.028; the latitude increments by 50 arcsec with each increment of +1 in file number. The antenna temperatures quoted in the maps have been corrected for ambient temperature losses, effects of Earth's atmosphere, and forward spillover and scattering losses. Included as a visual aid is the GIF image file 2quad.gif. This is the 39 deg. x 8.4 deg. map of the peak CO antenna temperature within the velocity interval -105 to 5 km/s. The GIF image was obtained from the FCRAO Web site, http://www-astro.phast.umass.edu/~fcrao/telescope/. A parallel survey of this outer Galaxy region is being conducted by DRAO to provide HI and radio continuum maps. The status of this survey may be checked at http://www.drao.nrc.ca/web/survey.shtml.
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S. Digel ADF J. Weiland ADF/ADC 1998 Jun 23 J_ApJS_115_241.xml UBV-{beta} Database for Case-Hamburg Northern and Southern Luminous Stars J/ApJS/115/271 J/ApJS/115/271 UBV-beta Database for LS Stars UBV-{beta} Database for Case-Hamburg Northern and Southern Luminous Stars B C Reed Astrophys. J. Suppl. Ser. 115 271 1998 1998ApJS..115..271R III/43 : Luminous Stars in the Southern Milky Way (Stephenson+ 1971) III/76 : Luminous Stars in the Northern Milky Way (Hardorp+ 1959-1965) V/92 : Photometric and Spectroscopic Databases for LSS Stars (Reed+ 1997) Milky Way MK spectral classification Photometry, UBV Photometry, uvby, beta Stars, luminous catalogs stars: early-type supergiants Between 1959 and 1971, the Hamburg and Warner and Swasey Observatories published a seven-volume survey listing intrinsically luminous stars (hereafter "LS" objects) - mostly OB stars, as well as a number of A, F, and G supergiants and Wolf-Rayet stars - within about ten degrees of the plane of the Milky Way to a limiting photographic magnitude of approximately 13.5. Based on objective-prism surveys of dispersion 580 Angstrom per millimeter at Hydrogen-gamma, these catalogs have served as starting points for numerous investigations of galactic structure and the characteristics of massive stars. Much fundamental data on the LS stars now exists distributed throughout the astronomical literature. This work describes a compilation of published photoelectric UBV-Beta photometry and spectral classifications nominally on the MK system for the LS stars, as well as an extensive cross-identification table linking LS numbers and other commonly-used identifiers such as HD, BD, CD, CPD and HR numbers. At this writing, the UBV-Beta portion of the database covers both the Northern and Southern LS stars, whereas MK classifications have as yet only been fully compiled for the Southern stars; compilation of MK types for the Northern LS stars is as yet incomplete, but ongoing.
UBV-beta data Alma-LS Alma LS number this number is the LSS (Luminous Southern Stars) when less than 6000 (the volume number is then zero), and starts from 6001 in Northern Milky Way. --- NoteFlag The '*' indicates a note in file notes.dat --- LS LS-North identification number the volume number as a roman numeral is in bytes 9-11, the declination zone in bytes 13-15, and the running number in bytes 17-20. This field is blank for Southern stars (i.e. Alma-LS < 6000) --- DM Cross-reference: BD, CD, or CP identification --- HD Number in HD catalog <III/135> --- Vmag V magnitude mag B-V color mag U-B color mag o_Vmag Number of UBV observations --- Hbeta H-Beta index mag o_Hbeta Number of Beta observations --- Notes Various notes --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec Ref Reference text --- Auth First author --- Rem Remarks/other identifications --- Cross-identifications Alma-LS Alma LS identifier: 1-13390 --- Vol Volume number if star is LS-North --- LSid Original LS-North declination zone and number; blank if LS-South --- BD Bonner DM (Cat. <I/119> and <I/122>) number --- CPD Cape Photographic DM (Cat. <I/108>) number --- CoD Cordoba DM (Cat. I</114>) number --- SAO SAO (Cat. <I/131>) number --- HD Henry Draper (Cat. <III/135>) number --- HR Bright Star (Cat. <V/50>) number --- Pmag LS-catalog photographic magnitude mag Notes Notes, including combined HD numbers. --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAds Right Ascension B1950 (deci-seconds) 0.1s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg LSclass LS-catalog objective-prism classification --- MK Classification Alma-LS Alma LS identifier (see ubvbeta.dat) --- LS LS-North identification (see ubvbeta.dat) --- DM Cross-reference: BD, CD, or CP identification --- HD Number in HD catalog <III/135> --- SpTemp Temperature Class --- SpLum Luminosity Class --- SpPec Spectral-luminosity peculiarities --- Disp Dispersion description - see LSNOTES --- Notes Notes and Remarks --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec Ref Reference --- Auth First author --- Rem Remarks/other identifications --- Notes flagged in ubvbeta.dat Alma-LS Alma LS identifier --- Text Text of note. the text starts by the photographic magnitude(s) given in the LSS catalog in parentheses; for LS-North stars, the text starts by the original LS-North identification numbers in square brackets. Numbers in square parentheses are reference numbers detailed in refs.dat. Note that KN refers to reference [1], Klare and Neckel (1977A&AS...27..215K) --- References quoted in notes.dat RefNum Reference number --- Text Text of Reference --- intro.txt Author's introduction Francois Ochsenbein CDS 1998 Oct 02 I am grateful to Arlene Nyman and the Inter-Library Loan staff of Alma College for securing a number of references. George Coyne, Pavel Mayer, Brian Skiff and Ana Orsatti kindly provided copies of a number of papers. Pat Carmody set up the anonymous ftp site. This research was supported by Research Corporation in the form of a Cottrell College Science Award, and by the Office of the Provost of Alma College. This research made use of the Simbad database, operated at CDS, Strasbourg, France. Author's address: B. Cameron Reed Department of Physics Alma College Alma, Michigan 48801 e-mail: reed@alma.edu (517) 463-7266 UNKNOWN UNKNOWN * 22-Jul-1998: Copied from ftp://sirius.mcs.alma.edu/pub (Version of 13 July 1998) * 02-Oct-1998: A new version was produced by C. Reed, following error reports. J_ApJS_115_271.xml Planetary nebulae in the NRAO VLA sky survey J/ApJS/117/361 J/ApJS/117/361 PNe in NRAO VLA Sky Survey Planetary nebulae in the NRAO VLA sky survey J J Condon D L Kaplan Astrophys. J. Suppl. Ser. 117 361 1998 1998ApJS..117..361C V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) Planetary nebulae Radio lines catalogs dust, extinction planetary nebulae: general radio continuum: ISM surveys The 1.4GHz NRAO VLA Sky Survey (NVSS) images and source catalog were used to detect radio emission from the 885 planetary nebulae north of J2000 declination {delta}=-40{deg} in the Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Cat. <V/84>). We identified 680 radio sources brighter than about S=2.5mJy/beam (equivalent to T~0.8K in the 45" FWHM NVSS beam) with planetary nebulae by coincidence with accurate optical positions measured from Digitized Sky Survey (DSS) images. Total extinction coefficients c at {lambda}=4861{AA} were calculated for the 429 planetary nebulae with available H{beta} fluxes and low free-free optical depths at 1.4GHz. The variation of c with Galactic latitude and longitude is consistent with the extinction being primarily interstellar and not intrinsic.
Optical and radio data PNG IAU name (PN G) --- RAh Optical right ascension (B1950) h RAm Optical right ascension (B1950) min RAs Optical right ascension (B1950) s DE- Optical declination sign (B1950) --- DEd Optical declination (B1950) deg DEm Optical declination (B1950) arcmin DEs Optical declination (B1950) arcsec RA2h Optical right ascension (J2000) h RA2m Optical right ascension (J2000) min RA2s Optical right ascension (J2000) s DE2- Optical declination sign (J2000) --- DE2d Optical declination (J2000) deg DE2m Optical declination (J2000) arcmin DE2s Optical declination (J2000) arcsec e_Pos Optical position uncertainty arcsec RArh Radio right ascension (J2000) h RArm Radio right ascension (J2000) min RArs Radio right ascension (J2000) s e_RArs rms uncertainty on RAr arcsec DEr- Radio declination sign (J2000) --- DErd Radio declination (J2000) deg DErm Radio declination (J2000) arcmin DErs Radio declination (J2000) arcsec e_DErs rms uncertainty on DEr arcsec l_S Limit flag on S --- S 1.4GHz flux-density peak mJy e_S rms uncertainty on S mJy PhiM Deconvolved Gaussian FWHM major axis arcsec l_Phim Limit flag on Phim --- Phim Deconvolved Gaussian FWHM minor axis arcsec c Total H{beta} extinction coefficient number=1 c = log[F_c_(Hbeta)/F(Hbeta)], where F_c_(Hbeta) is the Hbeta flux corrected for extinction --- Note Notes number=2 B: blanked radio image C: confused radio source E: very extended nebula whose flux density could not be measured *: individual note in notes.dat file --- Individual notes PNG IAU name (PN G) --- Note Text of the note --- James Marcout, Patricia Bauer CDS 1998 Sep 25 UNKNOWN UNKNOWN From ApJS electronic version J_ApJS_117_361.xml A three-position spectral line survey of Sagittarius B2 between 218 and 263 GHz. I. The observational data. J/ApJS/117/427 J/ApJS/117/427 Sgr B2 spectral survey A three-position spectral line survey of Sagittarius B2 between 218 and 263 GHz. I. The observational data. A Nummelin P Bergman A Hjalmarson P Friberg W M Irvine T J Millar M Ohishi S Saito Astrophys. J. Suppl. Ser. 117 427 1998 1998ApJS..117..427N Interstellar medium Radio lines Spectroscopy ISM: individual (Sagittarius B2) ISM: molecules line: identification surveys We have surveyed the frequency band 218.30-263.55GHz toward the core positions N and M and the quiescent cloud position NW in the Sgr B2 molecular cloud using the Swedish-ESO Submillimetre Telescope. In total 1730, 660, and 110 lines were detected in N, M, and NW, respectively, and 42 different molecular species were identified. The number of unidentified lines are 337, 51, and eight. Toward the N source, spectral line emission constitutes 22% of the total detected flux in the observed band, and complex organic molecules are the main contributors. Toward M, 14% of the broadband flux is caused by lines, and SO2 is here the dominant source of emission. NW is relatively poor in spectral lines and continuum. In this paper we present the spectra together with tables of suggested line identifications.
Sgr B2 17 47 20.4 -28 23 07
Line identifications toward Sagittarius B2(N) Line identifications toward Sagittarius B2(M) Line identifications toward Sagittarius B2(NW) Freq Observed frequency MHz Tmb Peak main-beam brightness temperature K DeltaV Velocity width km/s Ref Orion references number=1 B86: Blake et al., 1986ApJS...60..357B S85: Sutton et al., 1985ApJS...58..341S G91: Greaves & White, 1991A&AS...91..237G --- Iden Identification --- Rem Remarks --- Lines listed species by species El Element number=1 SO_2_ nu_2_=1 : SO_2_ in the {nu}_2_ = 1 Vibrational State NH_2_CN nu=1 : NH_2_CN in the v = 1 Vibrational State HC_3_N 1nu_5_ : HC_3_N in the 1{nu}_5_ Vibrational State HC_3_N 2nu_7_ : HC_3_N in the 2{nu}_7_ Vibrational State HC_3_N 1nu_6_ : HC_3_N in the 1{nu}_6_ Vibrational State HC_3_N 1nu_7_ : HC_3_N in the 1{nu}_7_ Vibrational State CH_3_OH vt=1 : CH_3_OH in the v_t_ = 1 Torsional State CH_3_OH vt=2 : CH_3_OH in the v_t_ = 2 Torsional State ^13^CH_3_OH vt=1 : ^13^CH_3_OH in the v_t_ = 1 Torsional State CH_3_CN nu_8_=1 : CH_3_CN in the {nu}_8_ = 1 Vibrational State CH_3_CHO vt=1 : CH_3_CHO in the v_t_ = 1 Torsional State CH_3_CHO vt=2 : CH_3_CHO in the v_t_ = 2 Torsional State C_2_H_3_CN 1nu11 : C_2_H_3_CN in the 1{nu}_11_ Vibrational State C_2_H_3_CN 1nu15 : C_2_H_3_CN in the 1{nu}_15_ Vibrational State C_2_H_3_CN 2nu11 : C_2_H_3_CN in the 2{nu}_11_ Vibrational State C_2_H_5_OH tran : C_2_H_5_OH in the tran Substates C_2_H_5_OH gau : C_2_H_5_OH in the gauche Substates CH_3_OCH_3_ For most transitions, the splitting of CH_3_OCH_3_ into its four torsional substates AA,EE, EA and AE has not been resolved, and for brevity we only list J_Ka,Kc_ in these cases --- RFreq Rest frequency MHz State State number=2 For HCN and HCO+, species For CH_3_OH, CH_3_SH, CH_3_NH_2_, CH_3_CHO, CH_3_OCHO: symmetry Symmetry : A, E; a = asymmetric state, s = symmetric state --- Trans Transition number=3 Type of transitions listed: J: SO+, HCN, HN^13^C, HCO, N_2_O, HCS+, OCS, NCNH+, _1_{SIGMA} diatomic species (CO, CS, SiO) J_F_: NO, NS N_J_: SO, C_2_H J_l_: HC_3_N J_K_: CH_3_CN, CH_3_C_2_H J_Ka,Kc_: HDO, SO_2_, H_2_CO, HNCO, HOCO+, H_2_CS+, CH2NH, c-C_3_H_2_, CH_2_CO, NH_2_CN, HCOOH, NH_2_CHO, c-c_2_H_4_O, C_2_H_3_CN, CH_3_OCHO, C_2_H_5_OH, CH_3_OCH_3_, C_2_H_5_CN J^p^_K_: CH_3_SH J^p^_Ka_: CH_3_OH, CH_3_NH_2_ J^p^_Ka,Kc_: CH_3_CHO N_Ka,Kc_: CH_2_CN --- n_Trans Note on transition number=4 F1 corresponds to J = (N + 3/2) -> (N + 1/2) F2 to J = (N + 1/2) -> (N - 1/2) a: a-Type Transitions b: b-type transitions c: c-type transitions a/b: a/b-Type transitions x: x-Type Transitions, See Plummer, Herbst, & De Lucia, 1987ApJ...318..873P For C_2_H_5_OH gau: + -> +; + -> -; - -> -; - -> + --- Eu Upper state energy number=5 ^33^SO: The E_u_ and A_ul_ values listed for are derived using the ^34^SO and SO values C_2_H_3_CN: In case of K-doublets, the Aul values listed refer to the individual transitions CH_3_OCH_3_: The rest frequencies and Aul values listed always refer to the subcomponent with highest statistical weight, EE, unless otherwise stated. K Aul A-coefficient number=5 ^33^SO: The E_u_ and A_ul_ values listed for are derived using the ^34^SO and SO values C_2_H_3_CN: In case of K-doublets, the Aul values listed refer to the individual transitions CH_3_OCH_3_: The rest frequencies and Aul values listed always refer to the subcomponent with highest statistical weight, EE, unless otherwise stated. s-1 N Observed integrated intensity at Sgr B2(N) number=6 Absorption lines have been indicated in the tables by negative integrated intensities K.km/s n_N Note number=7 u: up d: down a: line intensity incorrect due to emission in reference beam b: hyperfine-splitting partially resolved --- M Observed integrated intensity at Sgr B2(M)(6) K.km/s n_M Note number=7 u: up d: down a: line intensity incorrect due to emission in reference beam b: hyperfine-splitting partially resolved --- NW Observed integrated intensity at Sgr B2(NW)(6) K.km/s n_NW Note number=7 u: up d: down a: line intensity incorrect due to emission in reference beam b: hyperfine-splitting partially resolved --- Rem Remarks number=8 a: ambiguous b: blend o: overlap gnd: ground vibrational state of C_2_H_3_CN --- Unidentified lines Freq Observed frequency number=1 Assuming V_LSR_=+62km/s for all three positions. In case the U-line is common to N and M, the observed frequency listed is valid for N, and the frequency for M is noted in the Remarks column, if different. For the U-line that is common to M and NW (U247563) the listed observed frequency is for M. MHz N Observed integrated intensity at Sgr B2(N) K.km/s M Observed integrated intensity at Sgr B2(M) K.km/s NW Observed integrated intensity at Sgr B2(NW) number=2 Absorption lines have been indicated in the tables by negative integrated intensities K.km/s Rem Remarks number=3 S85: Detected by Sutton et al., 1985ApJS...58..341S B86: Detected by Blake et al., 1986ApJS...60..357B G91: Detected by Greaves & White, 1991A&AS...91..237G --- James Marcout, Patricia Bauer CDS 1999 Mar 09 UNKNOWN UNKNOWN From electronic version J_ApJS_117_427.xml A Deep Multicolor Survey. IV. The Electronic Stellar Catalog J/ApJS/119/189 J/ApJS/119/189 Deep Multicolor Survey. IV. A Deep Multicolor Survey. IV. The Electronic Stellar Catalog P S Osmer J D Kennefick P B Hall R F Green Astrophys. J. Suppl. Ser. 119 189 1998 1998ApJS..119..189O J/ApJS/104/185 : A deep multicolor survey. I. (Hall+ 1996) J/ApJ/462/614 : A deep multicolor survey. II (Hall+ 1996) J/AJ/114/2269 : A deep multicolor survey. III (Kennefick+ 1997) Galaxies, photometry QSOs Surveys catalogs galaxies: compact quasars: general stars: general surveys This stellar catalog contains 19,494 objects from the Deep Multicolor Survey (DMS) and results from follow-up spectroscopic observations of 234 objects in the catalog. The DMS is based on CCD imaging with the Mayall 4 m telescope in U, B, V, R', I75, and I86 and covers 0.83 deg^2 in six fields at high Galactic latitude. The survey reached 5 sigma limiting magnitudes of 22.1 in I86 to 23.8 in B. The catalog gives positions, magnitudes and error estimates, and classification codes in the six filter bands for all the objects. In addition, the survey is useful for the study of faint field galaxies and of faint stars at high Galactic latitude. Presented are tables that summarize the spectroscopic results for the 55 quasars, 44 compact narrow emission-line galaxies, and 135 stars in the DMS that we have confirmed to date. Also included are illustrations of all the spectra.
Field 01h of the Deep Multicolor Survey Field 10h of the Deep Multicolor Survey Field 14h of the Deep Multicolor Survey Field 17h of the Deep Multicolor Survey Field 21h of the Deep Multicolor Survey Field 22h of the Deep Multicolor Survey No Sequential number --- Field Field designation --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec x x coordinates on the image pix y y coordinates on the image pix Umag U magnitude mag e_Umag error estimate for U magnitude Error of 0.333 mag means that the magnitude value corresponds to the 3 sigma limit for that object. Also, an error value of -0.333 indicates that the object should have been detected in one of the frames but was not. Thus the measurement is being flagged as possibly subject to a non-statistical error. mag Bmag B magnitude mag e_Bmag error estimate for B magnitude mag Vmag V magnitude mag e_Vmag error estimate for V magnitude mag Rmag R magnitude mag e_Rmag error estimate for R magnitude mag I75mag I75 magnitude mag e_I75mag error estimate for I75 magnitude mag I86mag I86 magnitude mag e_I86mag error estimate for I86 magnitude mag u1 U magnitude filter classification code Refer to object classification codes from FOCAS for each filter and image. The codes are: s = star sf = fuzzy star Fs = forced star g = galaxy n = noise d = diffuse object l = long object u = unknown (not detected by FOCAS in both images of that field) x = no image available When an object was classified as a star in either or both images of a field, its classification was forced to star in each image - thus the Fs classification. No information was retained on the original classification in each image. An exception is objects used as PSF templates; these objects already had a "forced" flag present in FOCAS, and so the original classification was not overwritten. Most cases of "s" or "sf" in the catalog are objects of this sort. The other exceptions are all filters in the 01e and the B filter in the 10e field, for which only one image was available. In these cases, the classifications given are the original FOCAS classifications. --- u2 U magnitude image classification code --- b1 B magnitude filter classification code --- b2 B magnitude image classification code --- v1 V magnitude filter classification code --- v2 V magnitude image classification code --- r1 R magnitude filter classification code --- r2 R magnitude image classification code --- i1 I75 magnitude filter classification code --- i2 I75 magnitude image classification code --- I1 I86 magnitude filter classification code --- I2 I86 magnitude image classification code --- Comments Comments on individual objects Contains comments on individual objects. The codes are: q = quasar c = CNELG (compact narrow emission-line galaxy) s = star u = unknown (spectrum has too low S/N ratio to classify) The number following "q" or "c" is the redshift, with a "?" indicating an uncertain or unknown redshift. Other codes include "cr" for cosmic ray and "bp" for bad pixel followed by a filter and/or offset image code; i.e., "cr,u1" means a cosmic ray contaminates the object in the first U image. --- Spectroscopically Identified Quasars Spectroscopically Identified Compact Narrow Emission-Line Galaxies Name Quasars (table1.dat) and CNELG (table2.dat) --- ID Running number for the object and field identifier --- z Redshift --- u_z Uncertainty flag on z --- Umag U magnitude mag e_Umag error estimate for U magnitude Error of 0.333 mag means that the magnitude value corresponds to the 3 sigma limit for that object. Also, an error value of -0.333 indicates that the object should have been detected in one of the frames but was not. Thus the measurement is being flagged as possibly subject to a non-statistical error. mag Bmag B magnitude mag e_Bmag error estimate for B magnitude mag Vmag V magnitude mag e_Vmag error estimate for V magnitude mag Rmag R magnitude mag e_Rmag error estimate for R magnitude mag I75mag I75 magnitude mag e_I75mag error estimate for I75 magnitude mag I86mag I86 magnitude mag e_I86mag error estimate for I86 magnitude mag Spectroscopically Identified Stars ID Catalog Identification number --- Umag U magnitude mag e_Umag error estimate for U magnitude Error of 0.333 mag means that the magnitude value corresponds to the 3 sigma limit for that object. Also, an error value of -0.333 indicates that the object should have been detected in one of the frames but was not. Thus the measurement is being flagged as possibly subject to a non-statistical error. mag Bmag B magnitude mag e_Bmag error estimate for B magnitude mag Vmag V magnitude mag e_Vmag error estimate for V magnitude mag Rmag R magnitude mag e_Rmag error estimate for R magnitude mag I75mag I75 magnitude mag e_I75mag error estimate for I75 magnitude mag I86mag I86 magnitude mag e_I86mag error estimate for I86 magnitude mag Comments Comments on the spectral features or type of the star --- table1.ps Postscript version of table1 table2.ps Postscript version of table2 table3.ps Postscript version of table3 fig1.ps *Observed differential source counts fig2.ps *Log of the cumulative source counts fig3.ps V vs. B-V color-magnitude diagram for the stellar objects on the DMS Gail L. Schneider ADC/SSDOO 1999 Jun 11 Copied in May 1999 from ftp://ftp.astronomy.ohio-state.edu/pub/posmer/DMS4/ Patrick S. Osmer <posmer@astronomy.ohio-state.edu> J_ApJS_119_189.xml A complete redshift survey to the Zwicky catalog limit in a 2^h^x15{deg} region around 3C 273. J/ApJS/119/277 J/ApJS/119/277 -3.5<=DE<=8.5, 11.5<RA<13.5 redshift survey A complete redshift survey to the Zwicky catalog limit in a 2^h^x15{deg} region around 3C 273. N A Grogin M J Geller J P Huchra Astrophys. J. Suppl. Ser. 119 277 1998 1998ApJS..119..277G VII/203 : Las Campanas Redshift Survey (Shectman+ 1996) VII/4 : Abell and Zwicky Clusters of Galaxies (Abell+ 1974) Galaxy catalogs Redshifts catalogs galaxies: distances and redshifts large-scale structure of universe surveys We compile 1113 redshifts (648 new measurements, 465 from the literature) for Zwicky catalog galaxies (Cat. <VII/4>) in the region (-3.5{deg}<={delta}<=8.5{deg}, 11.5h<={alpha}<=13.5h). We include redshifts for 114 component objects in 78 Zwicky catalog multiplets. The redshift survey in this region is 99.5% complete to the Zwicky catalog limit, m_Zw_=15.7. It is 99.9% complete to m_Zw_=15.5, the CfA Redshift Survey (CfA2) magnitude limit. The survey region is adjacent to the northern portion of CfA2, overlaps the northernmost slice of the Las Campanas Redshift Survey (Cat. <VII/203>), includes the southern extent of the Virgo Cluster, and is roughly centered on the QSO 3C 273. As in other portions of the Zwicky catalog, bright and faint galaxies trace the same large-scale structure.
CGCG galaxies in the Survey region Name Name --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec mZW Zwicky magnitude mag HV Heliocentric velocity km/s e_HV rms uncertainty on HV km/s r_Vel Velocity source in refs.dat file --- n_Vel Note on Vel number=1 For New velocities, this paper. "a" denotes a fabtemp97 (absorption template) match "z" denotes a ztemp (absorption template) match "e" denotes a femtemp97 (emission template) match --- Com Comments --- Note b: See table3.dat file --- Velocity sources for the 3C 273 field redshift catalog (table 2) RefNo Number of the source of velocity --- BibCode BibCode --- Aut Author names --- Com Comments --- CGCG multiples in the Survey region Name Name --- m_Name Multiplicity index on Name --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec HV Heliocentric velocity km/s e_HV rms uncertainty on HV km/s r_Vel Velocity source in table2.dat file --- n_Vel Note on Vel number=1 For New velocities, this paper. "a" denotes a fabtemp97 (absorption template) match "z" denotes a ztemp (absorption template) match "e" denotes a femtemp97 (emission template) match --- Note b: Poor template correlation --- James Marcout, Patricia Bauer CDS 1999 Jan 19 UNKNOWN UNKNOWN From ApJS electronic version J_ApJS_119_277.xml Positions and flux densities of radio sources. J/ApJS/13/65 J/ApJS/13/65 Radio source flux densities at 750 & 1400MHz Positions and flux densities of radio sources. I I K Pauliny-Toth C M Wade D S Heeschen Astrophys. J. Suppl. Ser. 13 65 1966 1966ApJS...13...65P J/PASP/97/932 : 3CR Source Identifications (Spinrad 1985) Radio lines Radio sources Positions and flux densities at 750 and 1400MHz of 726 radio sources, measured with the 300-foot telescope, are given. Most of the positions are accurate to about +/-30" in each coordinate.
The measured positions and flux densities NRAO NRAO sequential number --- 3C 3C or 3CR number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s e_RAs rms uncertainty on right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec e_DEs rms uncertainty on declination (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg l_S750MHz Limit flag on S750MHz number=1 > stands for "larger or equal to" --- S750MHz Flux density at 750MHz Jy e_S750MHz rms uncertainty on S750MHz Jy l_S1400MHz Limit flag on S1400MHz number=1 > stands for "larger or equal to" --- S1400MHz Flux density at 1400MHz Jy e_S1400MHz rms uncertainty on S1400MHz Jy SI Spectral index --- e_SI rms uncertainty on SI --- Diam Source effective diameter number=2 No unit provided for this diameter, derived from the ratio of integrated to peak deflection. The diameters are very rough estimations and should be used with caution --- e_Diam rms uncertainty on Diam --- Notes Notes (in notes.dat file) --- Notes of table4.dat Note Note number --- Text Text of the note --- James Marcout, Patricia Bauer CDS 1998 Nov 13 UNKNOWN UNKNOWN Prepared via OCR at CDS, and proof-read by H. Andernach (heinz@astro.ugto.mx> J_ApJS_13_65.xml Faint blue objects at high galactic latitude. III. Palomar Schmidt field centered on Selected Area 28 J/ApJS/49/27 J/ApJS/49/27 Faint blue objects at high galactic latitude. III. Faint blue objects at high galactic latitude. III. Palomar Schmidt field centered on Selected Area 28 P D Usher K J Mitchell Astrophys. J. Suppl. Ser. 49 27 1982 1982ApJS...49...27U quasars: general stars: faint blue white dwarfs The third part of the list of ultraviolet excess objects is comprised of 1179 objects selected from a Palomar Schmidt three-color plate centered on Kapteyn Selected Area 28. The population belonging to color classes 1A, 1 and 1B should consist primarily of quasars and dwarfs and should be statistically complete to at least B = 18.5 mag.
Faint Blue Objects in Palomar Schmidt Field centered on SA 28 US Running number (US catalogue) --- CC Color class (1); it may include an uncertaintly flag [:] in byte 10. --- B Blue magnitude mag u_B uncertainty flag on B --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) number=2 values of 60 have been transformed arcsec Notes Comments. Abbreviations used: CG = Compact Galaxy C = confused sources ? = uncertainty E = edge zone R = further remarks (see paper) --- M.J. Wagner, Francois Ochsenbein CDS 1993 Jul 24 J_ApJS_49_27.xml An X-ray survey of clusters of galaxies. IV. A survey of southern clusters and a compilation of upper limits for both Abell and Southern clusters. J/ApJS/56/403 J/ApJS/56/403 X-ray survey of clusters of galaxies. IV. An X-ray survey of clusters of galaxies. IV. A survey of southern clusters and a compilation of upper limits for both Abell and Southern clusters. M P Kowalski M P Ulmer R G Cruddace K S Wood Astrophys. J. Suppl. Ser. 56 403 1984 1984ApJS...56..403K galaxies: clusters: general stars: luminosity function, mass function X-rays: sources The HEAO 1 A-1 X-ray survey of clusters of galaxies has been completed. We present X-ray error boxes and intensities or explicit upper limits for all clusters in the Abell catalog, and for the catalog of southern clusters and groups by Duus and Newell. The total of more than 3600 clusters surveyed makes this the most comprehensive survey of cluster X-ray emission to date. We have determined a subset of the southern sky catalog which is suitable for statistical studies and which may be combined with the Abell catalog.
Abell cluster X-ray sources Name Cluster name (Abell 1958) --- n_Name A "#" indicates new HEAO A-1 source --- n_Name Asterisk indicates cluster is not in Abell's statistical sample. --- RAdeg Right ascension 1950 of optical center deg DEdeg Declination 1950 of optical center deg RAdeg2 Right ascension 1950 of X-ray error box center deg DEdeg2 Declination 1950 of X-ray error box center deg RA1 90% confidence X-ray error box 1st corner RA deg DE1 90% confidence X-ray error box 1st corner DE deg RA2 90% confidence X-ray error box 2nd corner RA deg DE2 90% confidence X-ray error box 2nd corner DE deg RA3 90% confidence X-ray error box 3d corner RA deg DE3 90% confidence X-ray error box 3d corner DE deg RA4 90% confidence X-ray error box 4th corner RA deg DE4 90% confidence X-ray error box 4th corner DE deg Area Area of error box deg2 D Distance class (Abell 1958) --- R Richness class (Abell 1958) --- B-M Bautz-Morgan class from LV, unless noted. --- u_B-M A colon means uncertain classification --- R-S Revised Rood-Sastry class number=1 D<5: Revised Rood-Sastry class from Struble and Rood 1982 D=5: Revised Rood-Sastry class from Struble and Rood 1983 D=6: Revised Rood-Sastry class from Struble 1982 --- R-S2 Alternate classification under primary classification --- z Redshift --- e_z rms uncertainty on z. If no value is given, redshift error is assumed to be 0.0210 (Kowalski 1982) --- r_z Redshift reference number=2 (1) Abell 1958. (2) Corwin 1974. (3) Hoessel, Gunn, and Thuan 1980. (4) KUC. (5) LV. (6) Noonan 1981. (7) de Vaucouleurs 1961. (8) Hintzen, Scott, and McKee 1981. --- FX Flux in 10-3 A-1 counts cm-2 s-1. Data were summed in 1-day intervals (Kowalski 1982) 10-3ct/cm2/s e_FX rms uncertainty on FX 10-3ct/cm2/s log(LX) Log of the X-ray luminosity (2-6 keV). (Ho=75km/s/Mpc) 10-7W Other Other objects which could have been identified with this error box. --- Notes Individual notes number=3 Individual notes: (1) Distance, richness, and B-M classes from Sandage, Kristian, and Westphal 1976. Optical position is average of both spiral and elliptical components from de Vaucouleurs 1961. (2) Arp peculiar galaxy 102 is nearby (Biermann et al. 1981). Comparison shows that A2252 is the dominant source. (3) Error box contains globular cluster NGC 7089, but NGC 7089 is not the X-ray source (Grindlay 1980). (4) B-M class from Corwin 1974. (5) B-M classification discrepancy with Corwin 1974. LV classification adopted. (6) B-M class from Sandage, Kristian, and Westphal 1976. (7) Flux is not 3.5, but cluster is kept as an identified source. Paper I gave this identification to A2159, and Paper III gave it to A2152. Here we have assigned A2151 to the source according to our identification criteria (see text; Giovanelli 1983). (8) The error box is too far from the cluster for our association criteria, but HEAO-2 analysis shows that there is a source at the position of A2177. (9) Flux is not 3.5, but cluster is kept as an identified source. (10) Error box contains both A396 and AWM 7 (Schwartz et al. 1980). Comparison shows that A396 is the dominant source. (11) MKW 3 observed to have extended emission (Kriss et al. 1980). Comparison shows that A2063 is the dominant source. (12) HEAO-2 detected QSO 1028+313 at 5.5 X 10-12 ergs cm-2 s-1 (Zamorani et al. 1981), therefore half of the flux is from A1045. (13) Possible contamination with NGC 3227 (Marshall et al. 1980). Our HEAO-2 result shows that A992 is the dominant source. Monitor proportional counter data confirm this (Halpern 1980). (14) There is some source contamination with NGC 5548 (Piccinotti et al. 1982), but A-1 able to resolve cluster component. (15) X-ray source 3C 390.3 is nearby (Marshall et al. 1979), but is not the source. (16) X-ray source Mrk 501 is nearby (Piccinotti et al. 1982). Error box slightly outside cluster, but kept as the identification. (17) Error box slightly outside cluster, but kept as the identification (18) Revised Rood-Sastry class is "L10a". (19) Bimodal redshift distribution (Noonan 1981); redshift for A2319A chosen for cluster. Also, B-M classification discrepancy with Corwin 1974. LV classification adopted. --- Southern cluster X-ray sources Name Cluster name (DN) --- n_Name A "#" indicates new HEAO A-1 source --- n_Name Asterisk indicates cluster is not in Abell's statistical sample. --- RAdeg Right ascension 1950 of optical center (DN) deg DEdeg Declination 1950 of optical center (DN) deg RAdeg2 Right ascension 1950 of X-ray error box center deg DEdeg2 Declination 1950 of X-ray error box center deg RA1 90% confidence X-ray error box 1st corner RA deg DE1 90% confidence X-ray error box 1st corner DE deg RA2 90% confidence X-ray error box 2nd corner RA deg DE2 90% confidence X-ray error box 2nd corner DE deg RA3 90% confidence X-ray error box 3d corner RA deg DE3 90% confidence X-ray error box 3d corner DE deg RA4 90% confidence X-ray error box 4th corner RA deg DE4 90% confidence X-ray error box 4th corner DE deg Area Area of error box deg2 D Distance class (DN) --- T Concentration class (DN) --- B-M Bautz-Morgan class from White 1980 --- u_B-M A colon means uncertain classification --- R-S R-S classification (Lugger 1978) --- N Number of galaxies in the cluster uncorrected for field (DN) --- u_N Uncertainty flag on N --- z Redshift --- e_z rms uncertainty on z. If no value is given, redshift error is assumed to be 0.0210 (Kowalski 1982) --- r_z Redshift reference number=1 (1) DN: Duus and Newell 1977 (2) Chincarini, Tarenghi, and Bettis 1981. (3) Noonan 1981. (4) Yahil and Vidal 1977. (5) Sandage 1975a. (6) Zwicky distance class and redshift estimated directly from ESO films. (7) de Vaucouleurs, de Vaucouleurs, and Corwin 1976. (8) de Vaucouleurs 1975. (9) Dressler 1980b. --- FX Flux in 10-3 A-1 counts cm-2 s-1. Data were summed in 1-day intervals (Kowalski 1982) 10-3ct/cm2/s e_FX rms uncertainty on FX 10-3ct/cm2/s log(LX) Log of the X-ray luminosity (2-6 keV). (Ho=75km/s/Mpc) 10-7W Other Other objects which could have been identified with this error box. --- Notes Individual notes number=2 Individual notes: (1) Rose 5 (Rose 1976). (2) Rose 6. (3) Error box slightly outside cluster, but kept as the identification. (4) Very poor group (White 1980). (5) Ser 031-05 (Sersic 1974). (6) Ser 033-07. (7) Ser 040-06. (8) Snow 23 (Snow 1970). (9) Dev G8 (de Vaucouleurs 1975). X-ray Seyfert NGC 2997 is part of this group (Piccinotti et al. 1982). (10) Antilia group. (11) Abell cluster 1060 (Sandage 1975a). Revised R-S reference is C6 (Struble and Rood 1982). (12) Klem 15 (Klemola 1969). (13) Centaurus cluster. (14) Klem 21. Ex Hya is the source, not the cluster. (15) Klem 22. (16) Dev G4. Cen A (NGC 5128) is the source, not the cluster. (17) Sandage 1975. X-ray source MCG 6-30-15 is nearby (Marshall et al. 1980), but is not the source. (18) X-ray Seyfert ESO140G-43 is part of this group (Marshall et al. 1979). (19) There are two error boxes associated with this cluster. (20) Double cluster. Error box is slightly outside cluster, but kept as the identification. (21) Ser 137-02. Pavo cluster. There are two error boxes associated with this cluster. (22) Ser 138-07. Not given D/C classes by DN, but is on film #186 which they surveyed. (23) Ser 145-03. (24) Very poor group (White 1980). (25) Klem 34. X-ray source NGC 7163 is nearby (Marshall et al. 1979), but is not the source. (26) Ser 149-11. Not given D/C classes by DN, but is on film #146 which they surveyed. Error box slightly outside cluster, but kept as the identification. (27) Ser 151-02. X-ray source NGC 7213 is nearby (Piccinotti et al. 1982), but is not the source. (28) Rose 85. Error box slightly outside cluster, but kept as the identification. (29) Rose 107. NGC 7582 is part of Grus Quartet, G27 (de Vaucouleurs 1975). (30) Klem 44. --- Abell cluster survey n_Name Asterisk indicates cluster is not in Abell's statistical sample --- Name Name (Abell 1958). --- Code HEAO-1 A-1 letter code (see code table) --- RAdeg Right ascension 1950 of the optical center (Sastry and Rood 1971) deg DEdeg Declination 1950 of optical center (Sastry and Rood 1971) deg GLON Cluster optical center new galactic longitude (epoch 1950) deg GLAT Cluster optical center new galactic latitude (epoch 1950) deg l_Flux Limit flag on Flux --- Flux Flux or upper limit to flux in A-1 cts/cm2/s Data were summed in 1-day intervals for S and D clusters, and 4-day intervals for all other clusters (Kowalski 1982). ct/cm2/s l_log(LX) Limit flag on LX --- log(LX) Log of the X-ray luminosity or 2 upper limit (2-6 keV). (Ho=75km/s/Mpc). 10-7W z Redshift. For clusters with bimodal distributions (Noonan 1981) we choose one component: A2151B, A2241B, A2319A, and A2645B --- e_z rms uncertainty on z. If no value is given, error is assumed to be 0.0210 (Kowalski 1982). --- o_z Number of galaxies used to calculate measured redshifts. --- r_z Redshift reference number=1 Redshift reference. (1) Abell 1958. (2) Corwin 1974. (3) Hoessel, Gunn, and Thuan 1980. (4) KUC.Kowalski et al., 1983 (5) LV. Leir et al., 1977 (6) Noonan 1981. (7) de Vaucouleurs 1961. (8) Hintzen, Scott, and McKee 1981. --- Mag Magnitude of 10th brightest galaxy (Abell 1958). mag D Distance class (Abell 1958). --- R Richness class (Abell 1958). --- N Abell's counts of galaxies (Abell 1980). --- Radius Cluster optical radius in mm (LV). mm B-M Bautz-Morgan class. --- u_B-M A colon means uncertain classification. --- r_B-M B-M class reference number=2 Bautz-Morgan class reference. (1) LV. Leir et al., 1977 (2) Corwin 1974. (3) Sandage, Kristian, and Westphal 1976. (4) Bautz and Morgan 1970. (5) Bautz 1972. --- R-S Revised Rood-Sastry class. --- r_R-S Revised R-S class reference number=3 Revised Rood-Sastry class reference. (1) Struble and Rood 1982. (2) Struble and Rood 1983. (3) Struble 1982. --- R-S2 Alternate Revised R-S class. --- Southern cluster survey n_Name Asterisk indicates cluster is not in Abell's statistical sample --- Name Name (DN). number=1 DN identified 710 new clusters and groups, but included 248 previously identified clusters in their catalog. This table contains only 951 entries, because in some cases DN identified two clusters of different distances at the same coordinates. Our results are not capable of resolving the X-ray emission in such cases. --- Code HEAO-1 A-1 letter code (see code table) --- RAdeg Right ascension 1950 of optical center (DN) deg DEdeg Declination 1950 of optical center (DN) deg GLON Cluster optical center new galactic longitude deg GLAT Cluster optical center new galactic latitude deg l_Flux Limit flag on Flux --- Flux Flux or 1 sigma upper limit to flux in A-1 cts/cm2/s. Data were summed in 1-day intervals for S and D clusters, and 4-day intervals for all other clusters (Kowalski 1982). ct/cm2/s l_log(LX) Limit flag on LX --- log(LX) Log of the X-ray luminosity or 2 sigma upper limit (2-6 keV). (Ho=75km/s/Mpc). 10-7W z Redshift. --- e_z rms uncertainty on z. If no value is given, error is assumed to be 0.0210 (Kowalski 1982), except for values from Dressler 1980b which are 0.001. --- o_z Number of galaxies used to calculate measured redshifts. --- r_z Redshift reference number=2 Redshift reference: (1) DN. (2) Chincarini, Tarenghi, and Bettis 1981. (3) Noonan 1981. (4) Yahil and Vidal 1977. (5) Sandage 1975a. (6) Zwicky distance class and redshift estimated directly from ESO films. (7) de Vaucouleurs, de Vaucouleurs, and Corwin 1976. (8) de Vaucouleurs 1975. (9) Dressler 1980b. (10) (unexplained) (occurs four times) --- D Distance class (DN) number=3 Of the 782 clusters located on the 97 ESO films which DN surveyed, only 667 were given distance and concentration classes --- T Concentration class (DN) --- N Number of galaxies in the cluster uncorrected for field (DN) --- B-M Bautz-Morgan class. --- u_B-M A colon means uncertain classification. --- r_B-M B-M class reference number=4 Bautz-Morgan class reference: (1) White 1980 --- R-S Rood-Sastry class. --- r_R-S R-S class reference number=5 Rood-Sastry class reference: (1) Lugger 1978. (2) Struble and Rood 1982. Revised R-S class. --- L type confused regions for Abell clusters O type confused regions for Abell clusters n_Name Asterix indicates cluster is not in Abell's statistical sample --- Name Name (Abell 1958) --- RAdeg X-ray error box center right ascension (1950) deg DEdeg X-ray error box center declination (1950) deg RA1 90% confidence X-ray error box 1st corner RA deg DE1 90% confidence X-ray error box 1st corner DE deg RA2 90% confidence X-ray error box 2nd corner RA deg DE2 90% confidence X-ray error box 2nd corner DE deg RA3 90% confidence X-ray error box 3d corner RA deg DE3 90% confidence X-ray error box 3d corner DE deg RA4 90% confidence X-ray error box 4th corner RA deg DE4 90% confidence X-ray error box 4th corner DE deg Area Area of error box deg2 FX Flux in 10-3 A-1 counts cm-2 s-1. Data were summed in 1-day intervals (Kowalski 1982) 10-3ct/cm2/s e_FX rms uncertainty on FX 10-3ct/cm2/s *UWC confused regions for Abell clusters n_Name Asterix indicates cluster is not in Abell's statistical sample --- Name Name (Abell 1958) --- l_log(LX) Limit flag on LX --- log(LX) 2 sigma limit of the log of X-ray luminosity (2-6 keV) (Ho=75km/s/Mpc) 10-7W Code HEAO1 A-1 letter code (see code table) --- L type confused regions for southern clusters O type confused regions for southern clusters n_Name Asterix indicates cluster is not in Abell's statistical sample --- Name Name (DN) --- RAdeg X-ray error box center right ascension (1950) number=1 These error boxes were constructed in the data analysis, but they do not fulfill the criteria necessary for the association of the error box with the cluster (see text). In table6a, the error box is too large (L) In table6b, the error box does not overlap a 1 Abell radius circle which is concentric with the cluster center (O) deg DEdeg X-ray error box center declination (1950) number=1 These error boxes were constructed in the data analysis, but they do not fulfill the criteria necessary for the association of the error box with the cluster (see text). In table6a, the error box is too large (L) In table6b, the error box does not overlap a 1 Abell radius circle which is concentric with the cluster center (O) deg RA1 90% confidence X-ray error box 1st corner RA deg DE1 90% confidence X-ray error box 1st corner DE deg RA2 90% confidence X-ray error box 2nd corner RA deg DE2 90% confidence X-ray error box 2nd corner DE deg RA3 90% confidence X-ray error box 3d corner RA deg DE3 90% confidence X-ray error box 3d corner DE deg RA4 90% confidence X-ray error box 4th corner RA deg DE4 90% confidence X-ray error box 4th corner DE deg Area Area of error box deg2 FX Flux in 10-3 A-1 counts cm-2 s-1. Data were summed in 1-day intervals (Kowalski 1982) 10-3ct/cm2/s e_FX rms uncertainty on FX 10-3ct/cm2/s *UWC type confused regions for southern clusters n_Name Asterix indicates cluster is not in Abell's statistical sample --- Name Name (DN) --- l_log(LX) Limit flag on LX --- log(LX) 2 sigma limit of the log of X-ray luminosity (2-6 keV) (Ho=75km/s/Mpc) 10-7W Code HEAO1 A-1 letter code number=1 C: Clusters for which error boxes could not be defined. "C" clusters are regions with relatively strong emission (~1-3x10^-3^ct/cm2/s), but are sufficiently "confused" so that error boxes could not be obtained. D: Firmly identified X-ray clusters. When two or more clusters could be associated with a given source, the primary choice is given the letter "D" and alternates are given the letter "T" L: Clusters have error boxes that are "larger" than 1 deg2 O: Clusters have error boxes which do not "overlap" the circle of one Abell radius. S: Firmly identified X-ray clusters. S refers to a "single" identified cluster T: For firmly identified X-ray clusters, when two or more clusters could be associated with a given source, alternates are given the letter "T" U: Clusters for which error boxes could not be defined. Error box construction was not attempted for "U" clusters, for which "upper" limits are available only. W: Clusters for which error boxes could not be defined. "W" clusters have relatively "weak" emission, so that error box construction was not attempted. --- Patricia Bauer CDS 1995 Jan 30 UNKNOWN UNKNOWN The files were forwarded to CDS by Heinz J. Andernach (courtesy M.J. West, Aug. 1991) J_ApJS_56_403.xml Relativistic Free-Free Gaunt Factor of the Dense High-Temperature Stellar Plasma J/ApJS/63/661 J/ApJS/63/661 Relativistic Free-Free Gaunt Factor Relativistic Free-Free Gaunt Factor of the Dense High-Temperature Stellar Plasma M Nakagawa Y Kohyama N Itoh Astrophys. J. Suppl. Ser. 63 661 1987 1987ApJS...63..661N J/ApJ/382/636 : Rosseland mean free-free Gaunt factor (Itoh+ 1991) J/ApJS/74/291 : Relativistic Free-Free Gaunt Factor. II. (Itoh+ 1990) Atomic physics Opacities atomic processes opacities plasmas relativity The free-free Gaunt factor of the dense high-temperature stellar plasma is calculated by using the accurate relativistic cross section and is compared with the Gaunt factor derived by using Sommerfeld's exact nonrelativistic cross section. A wide range of electron degeneracy is accurately taken into account. Significant deviations from the nonrelativistic results are found for high-temperature cases. Results are presented in the form of extensive tables to facilitate applications.
*<<g_ff>>, degeneracy parameter {eta}=-6.0 <<g_ff>>, degeneracy parameter {eta}=-2.0 <<g_ff>>, degeneracy parameter {eta}= 0.0 <<g_ff>>, degeneracy parameter {eta}= 1.0 <<g_ff>>, degeneracy parameter {eta}= 2.0 <<g_ff>>, degeneracy parameter {eta}= 3.0 <<g_ff>>, degeneracy parameter {eta}= 5.0 <<g_ff>>, degeneracy parameter {eta}=10.0 <<g_ff>>, degeneracy parameter {eta}=20.0 <<g_ff>>, degeneracy parameter {eta}=40.0 Logu Log u, u=(h_bar_*{omega})/kT Log u, where u=(h_bar_*{omega})/kT, and {omega} is the angular frequency of the absorbed photon. --- Elem Element for Gaunt factor calculation The free-free Gaunt factor was calculated for the following: H - thermally averaged relativistic hydrogen He - thermally averaged relativistic helium G - thermally averaged nonrelativistic free-free Gaunt factor --- G-4.0 Gaunt factor, log({gamma}^2^)= -4.0 --- G-3.5 Gaunt factor, log({gamma}^2^)= -3.5 --- G-3.0 Gaunt factor, log({gamma}^2^)= -3.0 --- G-2.5 Gaunt factor, log({gamma}^2^)= -2.5 --- G-2.0 Gaunt factor, log({gamma}^2^)= -2.0 --- G-1.5 Gaunt factor, log({gamma}^2^)= -1.5 --- G-1.0 Gaunt factor, log({gamma}^2^)= -1.0 --- G-0.5 Gaunt factor, log({gamma}^2^)= -0.5 --- G+0.0 Gaunt factor, log({gamma}^2^)= 0.0 --- G+0.5 Gaunt factor, log({gamma}^2^)= 0.5 --- G+1.0 Gaunt factor, log({gamma}^2^)= 1.0 --- G+2.0 Gaunt factor, log({gamma}^2^)= 2.0 --- CDS 1998 Feb 06 AAS CD-ROM series, Volume 9, 1997 Lee E. Brotzman [ADS] 28-Aug-97 J_ApJS_63_661.xml The Case low-dispersion Northern Sky Survey. VI. A-F stars in a region near the North Galactic Pole J/ApJS/66/309 J/ApJS/66/309 The Case low-dispersion Northern Sky Survey. VI The Case low-dispersion Northern Sky Survey. VI. A-F stars in a region near the North Galactic Pole N Sanduleak Astrophys. J. Suppl. Ser. 66 309 1988 1988ApJS...66..309S J/ApJS/71/549 : The Case low-dispersion Northern Sky Survey. X. A-F (Pesch 1989) catalogs stars: spectral classification Positions, estimated magnitudes, and finding charts (when needed) are provided for 183 A-F stars (including both Population I and horizontal-branch stars) contained within the region 12h00m <R.A> <13h00m and +29.0 <decl. <+34.0. These stars, whose blue magnitudes range from 5.5 to 17.5, were identified on low-dispersion, objective-prism plates taken with the Burrell Schmidt telescope.
CASE North. Survey VI. Near NGP NO Running number . RAh 1950 Right Ascension h RAm 1950 Right Ascension min RAs 1950 Right Ascension s DE- 1950 Declination (sign) . DEd 1950 Declination deg DEm 1950 Declination arcmin m(b) apparent magnitude (eye estimate) mag var variabiblity remarks . SpCat Spectral category . Notes Name(s) / SpType / VarType . Francois Ochsenbein CDS 1993 Jan 04 J_ApJS_66_309.xml The case low-dispersion northern sky survey. VII. Late-type stars. J/ApJS/66/387 J/ApJS/66/387 The Case low-dispersion Northern Sky Survey. VII The case low-dispersion northern sky survey. VII. Late-type stars. N Sanduleak P Pesch Astrophys. J. Suppl. Ser. 66 387 1988 1988ApJS...66..387S stars: carbon stars: late-type stars: spectral classification *** No Description Available ***
Late-type stars CLS Name of the star --- RAh Right Ascension 1950 (hours) number=1 the accuracy of the position is 3arc in RA, and 6arcsec in declination h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) number=1 the accuracy of the position is 3arc in RA, and 6arcsec in declination - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Sp Spectral category: M = later than M5 C = Carbon star A colon indicates uncertainty --- R R magnitude based on (POSS)E prints mag u_R Uncertainty flag on R --- color Color indication, as: y = yellow (b-r < 1.5) r = red (1.5 < b-r < 2.5) vr = very red (b-r > 2.5) --- Notes Other names and remarks --- James Marcout, Francois Ochsenbein CDS 1994 Apr 06 UNKNOWN UNKNOWN Keypunched at CDS J_ApJS_66_387.xml The Clark Lake 30.9 MHz Galactic plane survey J/ApJS/68/715 J/ApJS/68/715 Clark Lake 30.9MHz survey The Clark Lake 30.9 MHz Galactic plane survey N E Kassim Astrophys. J. Suppl. Ser. 68 715 1988 1988ApJS...68..715K galaxies: structure Galaxy: general radio sources: general The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg<l<59deg, 84deg<l<97deg, and 133deg<l<250deg, with |b|<2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity confusion limited and varies from ~5Jy/beam in the inner Galaxy to ~1-2Jy/beam toward the outer Galaxy.
Source list Name Name based on its position in Galactic longitude and latitude --- RAh Right ascension 1950 h RAm Right ascension 1950 min DE- Declination sign --- DEd Declination 1950 deg D A 'p' indicates that the source is unresolved --- S30.9MHz Flux density at 30.9MHz --- Rem Remarks number=1 SNR Source is an identified Galactic supernova remnant W Source appears in Westerhout survey at 1390MHZ (Westerhout 1958) CUL Source appears in one of the Culgoora catalogs of sources at 80 or 160 MHz (Slee and Higgins 1973, 1975; Slee 1977) 3C Source appears in the Cambridge 3C catalog (Bennett 1963) 4C Source appears in the Cambridge 4C catalog (Gower, Scott, and Willis 1967; Pilkington and Scott, 1964) BG Source appears in the Bologna catalog of small-diameter sources (Fanti et al. 1974) C+C Source appears in the 408MHz list of small-diameter sources observed at Molonglo (Clark and Crawford 1974) --- Marie-Jose Wagner, Patricia Bauer CDS 1994 Dec 20 UNKNOWN UNKNOWN Keypunched at CDS J_ApJS_68_715.xml The centers of star formation in NGC 6334 and their stellar mass distributions J/ApJS/69/99 J/ApJS/69/99 NGC 6334 centers of star formation JHK photometry The centers of star formation in NGC 6334 and their stellar mass distributions S M Straw A R Hyland P J McGregor Astrophys. J. Suppl. Ser. 69 99 1989 1989ApJS...69...99S Clusters, open Photometry, infrared Supernova remnants HII regions ISM: molecules nebulae: individual (NGC 6334) open clusters and associations: general stars: formation stars: luminosity function, mass function We present near-infrared observations of specific sites of high-mass star formation activity in the giant H II region/molecular cloud complex NGC 6334. The observations consist of high-spatial resolution broad-band imaging, chopping photometry, and moderate-resolution spectra. The imaging observations provide full spatial sampling of the stellar population over a significant area of the cloud to a limit of K=13.5mag and reveal many faint red sources around the sites of recent high-mass star formation. We show that most of these sources are associated with the NGC 6334 molecular cloud and are not Galactic field sources. In the majority of the regions the embedded sources are primarily reddened main-sequence stars of low and intermediate mass though in three of the 11 regions studied there is a high proportion of objects showing H-K excesses which are therefore probably pre main-sequence. We identify the red objects in FIR-I as belonging to a very young compact cluster of ~1pc spatial extent. In FIR-V an unexpectedly large number of bright red sources are detected which have CO absorption at 2.3{mu}m. The probability that these objects are Galactic field sources is very low and if they are giant stars associated with NGC 6334 their implied ages (>10^9^yr) are inconsistent with the many indicators of extreme youth in this region. We propose that they form a hitherto unrecognized population of high-luminosity pre-main-sequence objects. Two objects with similar characteristics are also found in images of an area of the NGC 6334 molecular cloud to the north of FIR-V (SH-1). In FIR-V we also find evidence that the molecular outflow from the already known high-mass protostar has triggered intermediate-mass star formation via interaction with the local interstellar medium. Mass functions have been derived for the embedded stellar aggregates under the assumption that all sources lie on the main sequence unless otherwise indicated. The effect of a population of pre-main-sequence objects on the derived mass function slopes is shown to be small. Embedded aggregates in NGC 6334 have stellar mass distributions similar to those found both in young visible clusters and in other embedded clusters. This suggests that the slope of the mass function is relatively insensitive to conditions in the star formation environment and that the solar neighborhood value applies to star formation regions on scales as small as 1pc and of ages less than 10^7^yr.
NGC 6334 17 19 57.9 -35 57 47
Infrared sources in NGC 6334 IRS IRS name --- n_IRS Note on photometric results number=1 Asterisks indicate chopping photometry results; all other photometry is derived from the images. --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declinaiton (1950) deg DEm Declinaiton (1950) arcmin DEs Declinaiton (1950) arcsec Kmag K magnitude mag l_J-H Limit flag on J-H --- J-H J-H colour index mag l_H-K Limit flag on H-K --- H-K H-K colour index mag l_J-K Limit flag on J-K --- J-K J-K colour index mag K0 Derreddened K magnitude number=2 The derivation of dereddened K magnitudes and stellar masses are described in chap IIIb of the paper. mag LogM Stellar mass number=2 The derivation of dereddened K magnitudes and stellar masses are described in chap IIIb of the paper. [solMass] n_LogM Note on Mass number=3 *: Masses taken from Harvey and Gatley 1983ApJ...269..613H #: Masses derived from dereddening to pre-main-sequence tracks (Fig. 10) instead of ZAMS. --- Rem Remarks number=4 Edge: Source not covered by the J and/or H imaging area Opt: Source visible in the SRC-I plate Fore: Likely foreground source based on its near-infrared colors Ext: Extended source at K Neb: Probable knot in diffuse emission Back: Galactic background source (based on CVF data and/or reddening information) CVF: Spectrum obtained (Fig. 3). Abbreviations for previously reported photometry HG: Harvey and Gatley 1983ApJ...269..613H PF: Persi and Ferrari-Toniolo 1982A&A...112..292P BN: Becklin and Neugebauer 1974, Proc. of the Eighth ESLAB Symp. HII regions and the Galactic center, ed. A.F.M. Moorwood (Neuilly: ESRO), p. 39. BE: Braz and Epchtein 1982A&A...111...91B HW: Harvey and Wilding 1984ApJ...280L..19H --- Photometry and positions from supplementary imaging IRS IRS name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declinaiton (1950) deg DEm Declinaiton (1950) arcmin DEs Declinaiton (1950) arcsec Kmag K magnitude mag Marie-Jose Wagner, Patricia Bauer CDS 1997 May 02 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_69_99.xml Interstellar matter in early-type galaxies. I. IRAS flux densities J/ApJS/70/329 J/ApJS/70/329 IRAS flux densities for early-type galaxies Interstellar matter in early-type galaxies. I. IRAS flux densities G R Knapp P Guhathakurta D -W Kim M Jura Astrophys. J. Suppl. Ser. 70 329 1989 1989ApJS...70..329K galaxies: ISM infrared: sources (Abstract of the paper) The data from the IRAS satellite were co-added for about 1150 early-type galaxies with apparent magnitudes brighter than 14mag. At 60 and 100micro meter, about 45% of the ellipticals and 68% of the S0 galaxies are detected, showing that a large fraction of these galaxies contain cool interstellar matter.
IRAS flux densities for early-type galaxies NAME galaxy name 'N' for NGC, 'I' for IC, 'A' for anonymous others for ESO --- TYPE morphological type --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign . DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec BT total blue magnitude mag NOTE notes for the magnitude 'z'=magnitude taken from CGCG 'b' is not used in the paper, but used in "calc.for". '9' appears at N1574, probably an error. --- VEL heliocentric velocity See above description. km/s S12 observed equivalent point source flux density at 12um Jy e_S12 rms noise of above mJy S25 observed equivalent point source flux density at 25um Jy e_S25 rms noise of above mJy S60 observed equivalent point source flux density at 60um Jy e_S60 rms noise of above mJy S100 observed equivalent point source flux density at 100um Jy e_S100 rms noise of above mJy u_S uncertain because of confusion with a neighbouring galaxy etc. --- Koichi Nakajima CDS 1994 Mar 13 UNKNOWN UNKNOWN * The catalogue archived here is the Table 2 of the paper. Note that the flux data have been changed slightly from those in the paper. * Four typographic errors have been corrected, i.e. N5195, columns 48 and 57; N0560, column 74; and N0564, column 74. * Following description was originally attached to the software "calc.for": "The data for 1153 galaxies are in 'table2'. The columns are as in G.R.Knapp et al. 1989, ApJ Suppl 70, 329. The IR flux densities are in Jy, the 1 sigma noise in mJy. These are *NOT* corrected for the scale differences. The program 'calc.for' (see the source deck of 'calc.for') does this, rounds them off, and performs various manipulations to the optical magnitudes that the user may or may not care about. The redshifts are from RC2 (Sec.Ref.Cat., deVaucouleurs) RSA= Rev. Shapley-Ames, Sandage & Tammann 1981, Carnegie Davies et al. (see Burstein et al. 87, Ap.J.Suppl. 64,601 ('7 Samurai')) ZCAT = CfA redshift survey (J.P.Huchra, priv.comm.) " * The software "calc.for" needs two input files, i.e. "table2" and "types.dat". The latter is not archived here. * Performance of the software has not been well tested in CDS. The files were provided by courtesy of G.R. Knapp to H. Andernach; it was numbered A103 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 20-Oct-1993: First archived. 16-Apr-1994: Typographic errors in table2 were corrected. (The date of the latest archive, see the date of each file.) J_ApJS_70_329.xml The Case low-dispersion Northern Sky Survey. X. A-F stars in a region at intermediate galactic latitude primarily in Lynx and Leo Minor J/ApJS/71/549 J/ApJS/71/549 The Case low-dispersion Northern Sky Survey. X. A-F The Case low-dispersion Northern Sky Survey. X. A-F stars in a region at intermediate galactic latitude primarily in Lynx and Leo Minor P Pesch N Sanduleak Astrophys. J. Suppl. Ser. 71 549 1989 1989ApJS...71..549P J/ApJS/66/309 : The Case low-dispersion Northern Sky Survey. VI (Sanduleak 1988) stars: horizontal-branch Position, estimated magnitudes, and finding charts are provided for 540 A-F stars in the region 8h00m <R.A< 11h10m and +29.0 <Decl.<+43.0 (1950). The Galactic latitudes lie within the range +27 and +68. The A-F stars, with blue magnitudes between 14 and 17, were identified on low-dispersion objective-prism plates taken with the Burell Schmidt telescope. A large fraction of these A-F stars are extected to lebong to Population II.
CASE North. Survey X. A-F NO Running number . RAh 1950 Right Ascension h RAm 1950 Right Ascension min RAs 1950 Right Ascension s DE- 1950 Declination (sign) . DEd 1950 Declination deg DEm 1950 Declination arcmin m(b) apparent magnitude (eye estimate) mag SpCat Spectral category . Notes Other name(s) with type . Francois Ochsenbein CDS 1993 Jan 04 J_ApJS_71_549.xml The ultraviolet spectrum of eta Carinae J/ApJS/71/983 J/ApJS/71/983 The ultraviolet spectrum of eta Carinae The ultraviolet spectrum of eta Carinae R Viotti L Rossi A Cassatella A Altamore G B Baratta Astrophys. J. Suppl. Ser. 71 983 1989 1989ApJS...71..983V line: identification line: profiles stars: emission-line, Be stars: individual (eta Car) ultraviolet: spectra *** No Description Available ***
Spectrum Obs Observed wavelength (vacuum wavelength below 2000 A) 0.1nm u_Obs Uncertainty flag on Obs --- A/E Nature of the line: A=Absorption, E=Emission --- W Total width (in A) of the measured feature 0.1nm Weq Equivalent width (in A) or integrated line flux (in 10-15W/m2 = 10-12 erg.cm-2.s-1 not dereddened) of the absorption or emission feature respectively 0.1nm u_Weq Uncertainty flag on Weq --- Cont Estimated level of the continuum local to the feature (in 10-12 erg cm-2 s-1 A-1 not dereddened) 10-15W/m2 u_Cont Uncertainty flag on Cont --- ION Identification of the ion(s) contributing to the feature --- Lab Laboratory wavelength. 0.1nm n_Lab Note to Lab: K refers to a transition listed by Kurucz , or - indicates a second part (Lab2) --- Lab2 Second part of the line --- u_Lab2 Uncertainty flag on Lab2 --- Rem Remarks: I.S. = Interstellar Line; I.S.RED = Redshifted interstellar component; PGYG ABS = Violet shifted absorption of a P Cygni profile; EM PEAK = narrow emiss component; BROAD EM = broad emiss including any emiss peak; BLEND = blend of two or more lines; DB/MULT = double or multiple structure of the feature; FL = possible fluorescent line; see also notes to the table --- Francois Ochsenbein CDS 1993 Feb 19 J_ApJS_71_983.xml A 1.49 GHz atlas of the IRAS bright galaxy sample. J/ApJS/73/359 J/ApJS/73/359 1.49 GHz atlas of the IRAS bright galaxies A 1.49 GHz atlas of the IRAS bright galaxy sample. J J Condon G Helou D B Sanders B T Soifer Astrophys. J. Suppl. Ser. 73 359 1990 1990ApJS...73..359C Galaxies, IR Galaxies, radio Infrared sources Radio continuum galaxies: structure infrared: sources radio sources: galaxies This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).
A 1.49 GHz Atlas of IRAS Bright Galaxy Sample (5.5{deg} < Dec < 66{deg}) Name Name of galaxy number=1 This column gives the name of the galaxy. Note that for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. Full names of the galaxies as published (e.g. IRAS, NGC, UGC, MCG, etc.) have been shortened for convenience in the electronic version. --- Beam Restoring beamwidth (FWHM) number=2 The restoring beamwidth (FWHM) is given, in arcsec, in the beam column. Beamwidths of 48", 54", or 60" indicate D- or C/D-array maps from Condon (1987ApJS...65..485C) or Condon, Yin, and Burstein (1987ApJS...65..543C). Beamwidths of 15", 18", 21", or 24" indicate C array observations; beamwidths of 5", 6", 7", or 8" indicate B array observations; and beamwidths of 1.5", 1.8", 2.1", or 2.4" indicate A array observations. If there is no beam size value given, the flux density (see S1.49 and f_S1.49) is estimated from single-dish observations. Note that for N3735, N4038/9, N4490, N5194/5, N5427, N5678 and N7448 the beam size is approximate only. arcsec Contour Lowest contour plotted in published paper number=3 The contour column gives the value of n specifying the lowest contour plotted in the published paper, 2^(n/2)^ mJy per restoring beam solid angle. --- f_S1.49 Flagged if flux is estimated or uncertain number=4 These columns give the total 1.49 GHz flux density obtained by direct integration over the map and corrected for recognizable confusion. Usually the integration area is obvious from the published contour map; if not, it is described in the notes (also in published paper). The f_S1.49 column is marked with a "u" if the flux density is uncertain, or with an "e" if the flux density is estimated from single-dish observations. --- S1.49 Total 1.49 GHz corrected flux density number=4 These columns give the total 1.49 GHz flux density obtained by direct integration over the map and corrected for recognizable confusion. Usually the integration area is obvious from the published contour map; if not, it is described in the notes (also in published paper). The f_S1.49 column is marked with a "u" if the flux density is uncertain, or with an "e" if the flux density is estimated from single-dish observations. mJy RAh Right Ascension (B1950) (hour) number=5 These columns give the B1950 right ascension and declination of the source, in radians and in degrees. The radio position errors of all but the most extended sources are less than 1". Positions are radio positions unless the pos_flg column is marked with an "o" (19 objects), in which case the optical position is from LEDA (Lyon-Meudon Extragalactic Database). Where the pos_flg column is marked with an asterisk ('*'), the position is accurate to an extra decimal place (0.01s in right ascension and 0.1" in declination). Note that for 15 objects with missing positions in the original table we copied the radio position from the highest angular resolution measurement and flagged it with 'e' in the pos_flg column. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=5 These columns give the B1950 right ascension and declination of the source, in radians and in degrees. The radio position errors of all but the most extended sources are less than 1". Positions are radio positions unless the pos_flg column is marked with an "o" (19 objects), in which case the optical position is from LEDA (Lyon-Meudon Extragalactic Database). Where the pos_flg column is marked with an asterisk ('*'), the position is accurate to an extra decimal place (0.01s in right ascension and 0.1" in declination). Note that for 15 objects with missing positions in the original table we copied the radio position from the highest angular resolution measurement and flagged it with 'e' in the pos_flg column. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec pos_flg Flag denoting details of position number=5 These columns give the B1950 right ascension and declination of the source, in radians and in degrees. The radio position errors of all but the most extended sources are less than 1". Positions are radio positions unless the pos_flg column is marked with an "o" (19 objects), in which case the optical position is from LEDA (Lyon-Meudon Extragalactic Database). Where the pos_flg column is marked with an asterisk ('*'), the position is accurate to an extra decimal place (0.01s in right ascension and 0.1" in declination). Note that for 15 objects with missing positions in the original table we copied the radio position from the highest angular resolution measurement and flagged it with 'e' in the pos_flg column. --- oRA Radio minus infrared right ascension offset number=6 These columns give the radio-minus-infrared offset in right ascension and declination, in arcsec. arcsec oDE Radio minus infrared declination offset number=6 These columns give the radio-minus-infrared offset in right ascension and declination, in arcsec. arcsec S1.49p Peak flux density at 1.49 GHz number=7 These columns give the peak and integrated 1.49 flux densities, in mJy. These columns do not refer to the whole radio source but give fluxes of Gaussian fits to one or more components of the source. Where no integrated flux density is given, only the source peak was fitted. For full Gaussian fits down to the baseline level, the Gaussian integrated flux density is also listed. If a component was clearly resolved, its deconvolved major and minor FWHM diameters and its major-axis position angle are also given. mJy S1.49i Integrated flux density at 1.49 GHz number=7 These columns give the peak and integrated 1.49 flux densities, in mJy. These columns do not refer to the whole radio source but give fluxes of Gaussian fits to one or more components of the source. Where no integrated flux density is given, only the source peak was fitted. For full Gaussian fits down to the baseline level, the Gaussian integrated flux density is also listed. If a component was clearly resolved, its deconvolved major and minor FWHM diameters and its major-axis position angle are also given. mJy l_MajAxis Flagged if major axis is an upper limit number=8 These columns give parameters of Gaussian fits to one or more components of the source. The f_MajAxis column is marked with a '<' symbol if the major axis listed is an upper limit. The major axis and minor axis (deconvolved sizes, in arcsec) and the position angle (in degrees) are given when a component was clearly resolved. --- MajAxis FWHM major axis diameter number=8 These columns give parameters of Gaussian fits to one or more components of the source. The f_MajAxis column is marked with a '<' symbol if the major axis listed is an upper limit. The major axis and minor axis (deconvolved sizes, in arcsec) and the position angle (in degrees) are given when a component was clearly resolved. arcsec MinAxis FWHM minor axis diameter number=8 These columns give parameters of Gaussian fits to one or more components of the source. The f_MajAxis column is marked with a '<' symbol if the major axis listed is an upper limit. The major axis and minor axis (deconvolved sizes, in arcsec) and the position angle (in degrees) are given when a component was clearly resolved. arcsec PA Major axis position angle number=8 These columns give parameters of Gaussian fits to one or more components of the source. The f_MajAxis column is marked with a '<' symbol if the major axis listed is an upper limit. The major axis and minor axis (deconvolved sizes, in arcsec) and the position angle (in degrees) are given when a component was clearly resolved. deg Patricio Ortiz CDS 1999 Apr 01 UNKNOWN UNKNOWN "The catalogue was originally archived as A052 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_ApJS_73_359.xml The H II regions of M 101. I. An atlas of 1264 emission regions J/ApJS/73/661 J/ApJS/73/661 H II regions in M 101 The H II regions of M 101. I. An atlas of 1264 emission regions P Hodge M Gurwell J D Goldader R C Kennicutt Jr. Astrophys. J. Suppl. Ser. 73 661 1990 1990ApJS...73..661H Atlases H II regions galaxies: individual (M 101) HII regions A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.
M101 NGC 5457 14 03.3 +54 21
H II regions with positions from CCD frames H II regions with positions from image tube plates Seq Sequental number --- Frame CCD frame (table1) or image tube plate localisation (table2) --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec N1982 Chart number in Hodge & Kennicutt, 1983ApJ...267..563H --- N1969 Chart number in Hodge, 1969ApJS...18...73H --- H II regions within NGC complexes NGC NGC name --- HII HII region number --- Marie-Jose Wagner, Patricia Bauer CDS 1997 May 02 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_73_661.xml BVI photometry of globular clusters in M87 J/ApJS/73/671 J/ApJS/73/671 M87 globular clusters photometry BVI photometry of globular clusters in M87 J Couture W E Harris J W B Allwright Astrophys. J. Suppl. Ser. 73 671 1990 1990ApJS...73..671C galaxies: individual (M 87) globular clusters: general stars: abundances We present CCD photometry in B, V, and I for a sample of globular clusters in the Virgo central giant elliptical galaxy M87. Our measured sample comprises 270 objects brighter than V~23.4mag and with distances r>25" (>2kpc) from the center of the galaxy. In agreement with the recent study of Cohen, we find no detectable gradient of mean cluster color (metallicity) in (B-V) or (V-I) with radial distance. The cluster system does, however, display a large dispersion in color at any radius, corresponding to sigma([Fe/H])~0.6 about a mean metallicity (Fe/H]>~-1.1 according to our color index scale. The difference in mean color between the globular clusters and the underlying halo light of the galaxy itself, found previously by Strom and coworkers and by Cohen, shows up strongly in all of our color indices; we find virtually no clusters as red as mean color of the halo stars at any radius.
BVI photometry of M87 globular clusters SeqNum Starlike sequential number --- Xpos X position pix Ypos Y position pix Dist Distance arcsec Vmag V magnitude mag B-V (B-V) color mag V-I (V-I) color mag S6 Cross-identification with S6 catalog --- Marie-Jose Wagner, Patricia Bauer CDS 1995 Feb 27 UNKNOWN UNKNOWN Keypunched at CDS J_ApJS_73_671.xml EINSTEIN observations of galactic supernova remnants. J/ApJS/73/781 J/ApJS/73/781 X-ray observations of galactic Supernova Remnants EINSTEIN observations of galactic supernova remnants. F D Seward Astrophys. J. Suppl. Ser. 73 781 1990 1990ApJS...73..781S VII/211 : A Catalogue of Galactic Supernova Remnants Supernova remnants X-ray sources nebulae: supernova remnants X-rays: sources radio sources: general This paper summarizes the observations of Galactic supernova remnants with the imaging detectors of the Einstein Observatory. X-ray surface brightness contours of 47 remnants are shown together with gray-scale pictures. Count rates for these remnants have been derived and are listed for the HRI, IPC, and MPC detectors.
Einstein
SNR Count Rates in Einstein Detectors SNR_no SNR assigned number number=1 The first column contains the SNR assigned number; a number between 1 and 47, assigned in order of increasing right ascension. The SNR_no has a letter following it when this refers to an unresolved source (usually a pulsar) within the remnant. The common name for the supernova remnant can be found in the 'Name' column. --- GLON Galactic longitude from Green 1988 number=2 These columns give the galactic coordinates of the SNR from Green, D.A., (1988Ap&SS.148....3G), except for the Vela SNR where the position of the pulsar is used as the center of the remnant. For a more precise position, the table snr_indx.dat contains the right ascension and declination. deg GLAT Galactic latitude from Green 1988 number=2 These columns give the galactic coordinates of the SNR from Green, D.A., (1988Ap&SS.148....3G), except for the Vela SNR where the position of the pulsar is used as the center of the remnant. For a more precise position, the table snr_indx.dat contains the right ascension and declination. deg Name Common name of SNR number=1 The first column contains the SNR assigned number; a number between 1 and 47, assigned in order of increasing right ascension. The SNR_no has a letter following it when this refers to an unresolved source (usually a pulsar) within the remnant. The common name for the supernova remnant can be found in the 'Name' column. --- IPCcr Corrected IPC count rate number=3 These columns give the IPC (Imaging Proportional Counter) counts per second and error, after background subtraction. The count rates given are for the entire energy range of the IPC (pulse-height channels 1 to 15), integrated over the entire IPC field of view (~60' diameter). They have been corrected for vignetting, dead time, and scattering from the telescope mirror. A value of zero in the IPCcr column indicates that the source was not resolved in the IPC (see ipc_flag column). ct/s e_IPCcr Uncertainty on IPC count rate number=3 These columns give the IPC (Imaging Proportional Counter) counts per second and error, after background subtraction. The count rates given are for the entire energy range of the IPC (pulse-height channels 1 to 15), integrated over the entire IPC field of view (~60' diameter). They have been corrected for vignetting, dead time, and scattering from the telescope mirror. A value of zero in the IPCcr column indicates that the source was not resolved in the IPC (see ipc_flag column). ct/s f_IPCcr Flag for IPC counts number=4 This column gives a flag for the IPC count rate. The following flags are defined: (3) = includes surrounding diffuse emission > = count rate is a lower limit NRS = not resolved from other parts of SNR ave. = count rate is an average value --- HRIcr Corrected HRI count rate number=5 These columns give the HRI (High Resolution Imager) counts per second and error, after background subtraction. The count rates given have been integrated over the entire HRI field of view (~25' diameter) and corrected for vignetting, scattering in the telescope, and dead time. HRI rates have been corrected to January, 1979, the first use of HRI #3, the detector used for all SNR observations, and the closest time to the preflight calibration. A value of zero in the HRIcr column indicates no data or incomplete data for this remnant (see f_HRIcr column). ct/s e_HRIcr Uncertainty on HRI count rate number=5 These columns give the HRI (High Resolution Imager) counts per second and error, after background subtraction. The count rates given have been integrated over the entire HRI field of view (~25' diameter) and corrected for vignetting, scattering in the telescope, and dead time. HRI rates have been corrected to January, 1979, the first use of HRI #3, the detector used for all SNR observations, and the closest time to the preflight calibration. A value of zero in the HRIcr column indicates no data or incomplete data for this remnant (see f_HRIcr column). ct/s f_HRIcr Flag for HRI counts number=6 This column gives a flag for the HRI count rate. The following flags are defined: (2) = estimated from partial HRI observation and HRI/IPC ratio (3) = includes surrounding diffuse emission INC = incomplete data, much of SNR not observed ND = no data, not observed ave. = count rate is an average value --- MPCcr Corrected MPC count rate number=7 These columns give the MPC (Monitor Proportional Counter) counts per second and error, after background subtraction in channels 1-6 (1-10 keV). A value of zero in the MPCcr indicates the source was not resolved (see f_MPCcr column). ct/s e_MPCcr Uncertainty on MPC count rate number=7 These columns give the MPC (Monitor Proportional Counter) counts per second and error, after background subtraction in channels 1-6 (1-10 keV). A value of zero in the MPCcr indicates the source was not resolved (see f_MPCcr column). ct/s f_MPCcr Flag for MPC counts number=8 This column gives a flag for the MPC count rate. The following flags are defined: (3) = includes surrounding diffuse emission > = count rate is a lower limit NRB = not resolved from nearby bright sources NRS = not resolved from other parts of SNR ave. = count rate is an average value --- class Classification of the X-ray morphology number=9 This column gives the classification of the X-ray morphology. More than one classification may be presented for a given supernova remnant. The following classifications are used: S = shell F = filled center, plerionic IR = irregular CO = central object NI = neutron star, isolated NB = neutron star in binary system --- comments Miscellaneous comments number=10 This column gives miscellaneous comments pertaining to the supernova remnant. An "INC" indicates that there is incomplete data, much of SNR was not observed. --- Index to FITS Images of SNR Available on Tape File FITS tape file number number=1 This column contains the FITS tape file number on the tape. The first 74 files contain smoothed images, with the smooth described in the columns "width" and "f_width". Files 75 to 148 contain a set of background-subtracted images which have not been smoothed, with which the user can apply his or her own image-processing techniques. These images were used to make those in files 1 - 74. For example: the image of CTA 1 (smoothed file = #34) before smoothing is located in tape file 74 + 34 = 108. The maximum value of array elements has usually been set to be 32000 for files 75 - 148. --- GLON Galactic Longitude from Green 1988 number=2 The galactic coordinates from Green, D.A. (1988Ap&SS.148....3G), are given in the columns GLON and GLAT. The "Name" column gives the common name of the supernova remnant. Also given in this column is information to distinguish the array from other arrays of the same source. For instance, a given supernova remnant may have different files for different energy bands. See the "energy" column for details on the energy band used. See the "Seqno" column to determine which instrument was used. deg GLAT Galactic Latitude from Green 1988 number=2 The galactic coordinates from Green, D.A. (1988Ap&SS.148....3G), are given in the columns GLON and GLAT. The "Name" column gives the common name of the supernova remnant. Also given in this column is information to distinguish the array from other arrays of the same source. For instance, a given supernova remnant may have different files for different energy bands. See the "energy" column for details on the energy band used. See the "Seqno" column to determine which instrument was used. deg Name Common name number=2 The galactic coordinates from Green, D.A. (1988Ap&SS.148....3G), are given in the columns GLON and GLAT. The "Name" column gives the common name of the supernova remnant. Also given in this column is information to distinguish the array from other arrays of the same source. For instance, a given supernova remnant may have different files for different energy bands. See the "energy" column for details on the energy band used. See the "Seqno" column to determine which instrument was used. --- ArrSize Number of pixels in array number=3 These columns give the number of pixels in the image array, and the pixel size in arcseconds. --- PixSize Pixel size number=3 These columns give the number of pixels in the image array, and the pixel size in arcseconds. arcsec RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec width Width of the function used for smooth number=4 The "width" column gives the width of the Gaussian function, in arcseconds, used to smooth the data. This column contains a 0 when the smoothing was done by decon or when no smoothing was applied. The "f_width" indicates what kind of smoothing was used. The following flags are defined: decon = maximum entropy deconvolution gauss = Gaussian smoothing none = no smoothing arcsec f_width Flag determining kind of smoothing number=4 The "width" column gives the width of the Gaussian function, in arcseconds, used to smooth the data. This column contains a 0 when the smoothing was done by decon or when no smoothing was applied. The "f_width" indicates what kind of smoothing was used. The following flags are defined: decon = maximum entropy deconvolution gauss = Gaussian smoothing none = no smoothing --- Seqno Einstein fields used to make the figure number=5 This column lists the Einstein fields used to make the figure. The sequence numbers are The Einstein sequence number is a two to five digit number which uniquely identifies the observation. The numbers were assigned at the time of proposal submission. An "I" before the sequence number indicates that the field was observed with the IPC; an "H" before the sequence number indicates that the field was observed with the HRI. When multiple sequence numbers are listed and were observed with the same instrument, the leading letter was omitted for the latter sequence numbers. --- max_val Maximum data value in the array number=6 The "max_val" column gives the maximum value of the array. The "energy" column gives the range of IPC data included in the figure (in keV). The HRI energy range is always 0.15-4 keV, with maximum response at 0.2-2.0 keV; this is indicated by a (1) in the "energy" column. --- energy Energy range of IPC data included in the figure number=6 The "max_val" column gives the maximum value of the array. The "energy" column gives the range of IPC data included in the figure (in keV). The HRI energy range is always 0.15-4 keV, with maximum response at 0.2-2.0 keV; this is indicated by a (1) in the "energy" column. keV Unresolved X-ray Sources Within or Nearby the SNR RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Name Common name of the SNR --- Instr Instrument used in the observation number=1 The instrument used in the observation will either be the IPC (Imaging Proportional Counter) or the HRI (High Resolution Imager). --- Seqno Sequence number of the observation number=2 The sequence number is a two to five digit number which uniquely identifies the observation. The numbers were assigned sequentially at the time of proposal submission. --- Ctrate Total counting rates number=3 This column gives the total counting rates (in units of counts per second). All energy channels of the IPC (1-15) are included and corrections have been made for mirror-scattering and dead time. For the HRI, the energy range is always 0.15-4 keV, with maximum response at 0.2-2.0 keV, and these corrections have also been made. ct/s loc_flg Flag for where source is located in relation to SNR number=4 This column gives a flag indicating where the source is located, in relation to the SNR. The following flags are defined: O = source lies outside the boundary of the SNR I = source lies inside the boundary of the SNR C = source lies at the approximate center of the SNR --- ID Identification of the source, when known number=5 This columns gives the optical identification of the source, when known. If no identification is known, "no ID" will appear in the column, along with any miscellaneous comments such as "extended" or "variable." --- Patricio Ortiz CDS 1999 Apr 06 UNKNOWN UNKNOWN Prepared from the tables available at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) J_ApJS_73_781.xml A catalog of small-diameter radio sources in the Galactic plane J/ApJS/74/181 J/ApJS/74/181 Small-diameter radiosources catalogue A catalog of small-diameter radio sources in the Galactic plane S Zoonematkermani D J Helfand R H Becker R L White R A Perley Astrophys. J. Suppl. Ser. 74 181 1990 1990ApJS...74..181Z Galactic plane Radio sources Surveys radio sources: general A survey of the Galactic plane in the longitude range -20deg=<l<=120deg for Galactic latitudes |b|=<0.8deg has been carried out at 1400MHz using the VLA in the B configuration. We present here a catalog of the 1992 discrete sources detected in this survey which is ~75% complete to a limiting peak flux density of 25mJy for sources smaller than ~20" in diameter, although sources as faint as 8mJy and as large as 90" are also included. The catalog includes for each entry a position accurate to ~<3", peak and integrated flux densities, source extent, and information on counterparts both from earlier radio surveys of the plane (for which a comprehensive bibliography is included) and from the IRAS point source catalog. An extensive analysis of the integrity and completeness of the survey is presented here: in separate publications, we discuss the source content of the survey as derived from statistical analysis of the spatial distribution of the sources and from radio, optical and infrared follow up observations .
Catalog of compact 20 centimeter sources Name Source name based on its Galactic coordinates --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Speak Peak flux density mJy Sint Integrated flux density mJy n_Sint A '+' indicates extended sources which had obviously non-Gaussian brightness distributions number=1 For these sources, a flux density was determined by summing the intensity within a polygon enclosing the source. --- Size Source diameter arcsec Offset Off-axis angle arcsec Comment Comments number=2 Annotation translations: * Marks a set of related sources Rxx Catalogued in Reich et al. (1984A&AS...58..197R); xx = source number INT=xxx Integrated flux density (xxx in mJy) derived from a region of diffuse emission surrounding the source A Catalogued in Altenhoff et al. 6cm list (1979A&AS...35...23A), Hxx Catalogued in Handa et al. (1987PASJ...39..709H); xx = source number F5=xxx, F15=xxx Flux densities (xxx) recorded at 5GHz and 15 GHz, respectively, in VLA observations of Fich (1986AJ.....92..787F) TX=xxx Catalogued in Texas 365 MHz interferometer survey (Douglas et al. 1980PAUTx..17....1D) with flux density (xxx) in mJy. Flux densities reported here are from a preliminary version of the catalogue and are subject to revision by ~10%. SNRxx.x+x.x Supernova remnant Gxx.x+x.x form catalog of Green 1989 (1989A&AS...78..277G) RL Recombination lines observed from this direction by Lockman (1989ApJS...71..469L) and/or Caswell and Haynes (1987A&A...171..261C) FU=LCXU Follow up observations exist at 20cmR (L), 6cm (C), 3.5cm (X), and/or 2cm (U), see Table 8 and paper II for results. I Coincident with an entry in the IRAS Point Source Catalog (see White R.L. et al., in preparation for details; see Cat. <II/125>) X( ) Coincident to <=60" with source in Einstein IPC catalog (with name if known) PNxxx+x.x Entry in Strasbourg Planetary Nebula Catalog MCG Matching entry in Morphological Catalog of Galaxies (Cat. <VII/62>, <VII/100>) Sxx.xx Star in the SAO or HST Guide Star Catalog (GSC) with magnitude (xx.xx) (Cats. <I/131> and <I/220>) LO Object was observed at Lick Observatory --- Simona Mei, Patricia Bauer CDS 1994 Dec 19 UNKNOWN UNKNOWN * 19-Dec-1994: OCR'ed at CDS * 22-May-1998: Thanks to H. Andernach <heinz@polaris.astro.ugto.mx> 33 rows were corrected, most of the errors being missing "I" flags in the Comment column. J_ApJS_74_181.xml Observations of double stars and new pairs. XIV J/ApJS/74/275 J/ApJS/74/275 Observations of double stars XIV Observations of double stars and new pairs. XIV W D Heintz Astrophys. J. Suppl. Ser. 74 275 1990 1990ApJS...74..275H binaries: visual Visual and photographic measures listed for 1550 pairs were obtained in the time 1987.07-1989.90; they include 194 new double stars.
Table 2 + Table 4 Name Name of system --- RAh Right Ascension 2000 (hours) h RAdm Right Ascension 2000 (deci-minutes) 0.1min DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin Ep Observation date (offset 1980) yr PA Position angle deg u_PA Uncertainty flag on PA, "r" for round image, "s" for single --- Sep Separation between the components arcsec u_Sep Uncertainty flag on Sep --- n Number of nights --- Inst Instrument: S = Swarthmore 61cm refractor T = Cerro Tololo Interamerican Obs., mainly 1m refravctor L = Lowell 60cm telescope --- Note (magnitudes or components) --- Notes to tables Name Name of system (blank for a continuation) --- Text Text of note --- M.J. Wagner, Francois Ochsenbein CDS 1993 Nov 03 UNKNOWN UNKNOWN Table 2 and Table 4 have been keypunched at CDS, and combined into a single table J_ApJS_74_275.xml Relativistic Free-Free Gaunt Factor of the Dense High-Temperature Stellar Plasma. II. Carbon and Oxygen Plasmas J/ApJS/74/291 J/ApJS/74/291 Relativistic Free-Free Gaunt Factor. II. Relativistic Free-Free Gaunt Factor of the Dense High-Temperature Stellar Plasma. II. Carbon and Oxygen Plasmas N Itoh K Kojo M Nakagawa Astrophys. J. Suppl. Ser. 74 291 1990 1990ApJS...74..291I J/ApJS/63/661 : Relativistic Free-Free Gaunt Factor (Nakagawa+ 1987) J/ApJ/382/636 : Rosseland mean free-free Gaunt factor (Itoh+ 1991) Atomic physics Opacities atomic processes opacities plasmas relativity The pure Coulomb free-free Gaunt factors of the dense high-temperature carbon and oxygen plasmas are calculated by using the accurate relativistic cross section and are compared with the Gaunt factors derived by using Sommerfeld's exact nonrelativistic cross section. A wide range of electron degeneracy is accurately taken into account. Effects from resonances in the free electron density of states are not included. Dramatic deviations from the nonrelativistic results are found for high-temperature cases. Results are presented in the form of extensive tables to facilitate applications.
*<<g_ff>>, degeneracy parameter {eta}=-6.0 <<g_ff>>, degeneracy parameter {eta}=-2.0 <<g_ff>>, degeneracy parameter {eta}= 0.0 <<g_ff>>, degeneracy parameter {eta}= 1.0 <<g_ff>>, degeneracy parameter {eta}= 2.0 <<g_ff>>, degeneracy parameter {eta}= 3.0 <<g_ff>>, degeneracy parameter {eta}= 5.0 <<g_ff>>, degeneracy parameter {eta}=10.0 <<g_ff>>, degeneracy parameter {eta}=20.0 <<g_ff>>, degeneracy parameter {eta}=40.0 Logu Log u, u=(h_bar_*{omega})/kT Log u, where u=(h_bar_*{omega})/kT, and {omega} is the angular frequency of the absorbed photon. --- Elem Element for Gaunt factor calculation The free-free Gaunt factor was calculated for the following: H - thermally averaged relativistic carbon He - thermally averaged relativistic oxygen G - thermally averaged nonrelativistic free-free Gaunt factor --- G-4.0 Gaunt factor, log({gamma}^2^)= -4.0 --- G-3.5 Gaunt factor, log({gamma}^2^)= -3.5 --- G-3.0 Gaunt factor, log({gamma}^2^)= -3.0 --- G-2.5 Gaunt factor, log({gamma}^2^)= -2.5 --- G-2.0 Gaunt factor, log({gamma}^2^)= -2.0 --- G-1.5 Gaunt factor, log({gamma}^2^)= -1.5 --- G-1.0 Gaunt factor, log({gamma}^2^)= -1.0 --- G-0.5 Gaunt factor, log({gamma}^2^)= -0.5 --- G+0.0 Gaunt factor, log({gamma}^2^)= 0.0 --- G+0.5 Gaunt factor, log({gamma}^2^)= 0.5 --- CDS 1998 Feb 06 AAS CD-ROM series, Volume 9, 1997 Lee E. Brotzman [ADS] 28-Aug-97 J_ApJS_74_291.xml The supergalactic plane redshift survey J/ApJS/75/241 J/ApJS/75/241 The supergalactic plane redshift survey The supergalactic plane redshift survey A Dressler Astrophys. J. Suppl. Ser. 75 241 1991 1991ApJS...75..241D galaxies: clusters: general galaxies: distances and redshifts *** No Description Available ***
The catalogue SPS Running number --- ESO ESO Catalogue designation --- RAH 1950 right ascension h RAM 1950 right ascension min RAS 1950 right ascension s DE- 1950 Declination sign --- DED 1950 Declination deg DEM 1950 Declination arcmin DES 1950 Declination arcsec SLon Supergalactic longitude deg SLat Supergalactic latitude deg a Major axis diameter arcmin b Minor axis diameter arcmin BT Total B magnitude from ESO-LV Catalogue mag Vel Heliocentric radial velocity (cz) km/s sc spectral characteristics (origin of spectrum) See the publication. --- Type Morphological type (from ESO) --- NAME Alternative name of the galaxy --- Francois Ochsenbein CDS 1992 Dec 31 J_ApJS_75_241.xml Optical spectroscopy of Magellanic Cloud planetary nebulae. I. J/ApJS/75/407 J/ApJS/75/407 LMC & SMC PNe optical spectroscopy. I Optical spectroscopy of Magellanic Cloud planetary nebulae. I. S J Meatheringham M A Dopita Astrophys. J. Suppl. Ser. 75 407 1991 1991ApJS...75..407M J/MNRAS/234/583 : Abundances in Magellanic Cloud planetary nebulae J/ApJS/76/1085 : PNe Magellanic Cloud optical spectroscopy. II J/ApJS/83/87 : PNe Magellanic Cloud optical spectroscopy. III J/A+AS/121/407 : LMC planetary nebulae positions (Leisy+ 1997) Magellanic Clouds Nebulae, planetary Spectroscopy Magellanic Clouds nebulae: planetary We present optical spectroscopy in the range 3300-7400A for a total of 30 planetary nebulae in the LMC and 11 in the SMC, with measurements of line intensities down to ~1% of H{beta}. Agreement with other authors is on the whole excellent, especially for lines >+10%-20% of H{beta}. Reddening estimates from Balmer line ratios have been determined, and the line intensities dereddened accordingly. Nebular [O III] electron temperature and, where measurable, [N II] temperatures and [S II] densities are given. [O II] electron densities are recalculated using appropriate electron temperatures. A number of spectra exhibit interesting spectral features (including symbiotic-type profiles, unidentified emission lines, and nonsimple Balmer decrements). These objects are discussed in some detail. Zanstra temperatures are derived for a total of 25 objects possessing detectable stellar continua. These temperatures are in agreement with the few published values from various methods, and preliminary photoionization modeling of this sample. The homogeneity and size of the sample make it possible to investigate several interesting correlations between measured parameters.
Corrected line intensities Lambda Wavelength 0.1nm ID Identification of line --- PN Planetary nebula name --- I(Lambda) Measured line intensity (I(H{beta})=100) --- n_I(Lambda) n: No ; s: Saturated --- u_I(Lambda) Uncertainty flag on I(Lambda) --- Patricia Bauer CDS 1996 Oct 03 Pierre Leisy <leisy@iap.fr> J_ApJS_75_407.xml The Fourth MIT-Green Bank 5GHz Survey J/ApJS/75/801 J/ApJS/75/801 MGIV The Fourth MIT-Green Bank 5GHz Survey M Griffith G Langston M Heflin S Conner B Burke Astrophys. J. Suppl. Ser. 75 801 1991 1991ApJS...75..801G VIII/38 : The Parkes-MIT-NRAO 4.85GHz (PMN) Surveys (Griffith+ 1993-1996) Radio sources Surveys radio sources: general radio sources: identifications The MIT-Green Bank IV (MG IV) 5 GHz survey covers 0.504 sr of sky in the right ascension range 15.5 to 2.5 hours, between +37.00 and +50.98 degrees declination (B1950). The final MG IV catalog contains 3427 sources detected with a signal-to-noise ratio greater than 5. The catalog was produced from two separate north and south surveys with the National Radio Astronomy Observatory (NRAO) 91m transit telescope. The north survey was produced from data collected while scanning the telescope north from +39.0 to +50.98 degrees declination and the south survey from data collected from scans from +48.98 to +37.00 degrees declination. The completeness and reliability of the final source list is checked by examination of north and south source lists in a twice observed comparison region, lying between +39.15 and +48.83 degrees declination and excluding the area between +/-10 degrees Galactic latitude. The comparison region covers 0.270 sr of sky and contains 1094 sources. In this region, the MG IV catalog contains 423 sources brighter than 90 mJy and is shown to be 99.1 +/- 1.2% complete at this flux density level. Spectral indices are computed for sources identified in the NRAO 1400 MHz Survey (published by Condon and Broderick in 1985). A comparison of the spectral index distributions between +/- 10 and outside of +/- 10 degrees Galactic latitude is presented. Nomenclature Note: The source names are derived from the J2000 coordinates; a 'J' was added in front of this name to comply with IAU recommendations on designations, and the suffix 'a' or 'b' was added for 132 sources with identical names.
JMG IV source list Name The source names are derived from the J2000 coordinates (see "Nomenclature Note" section above) --- RAh right ascension J2000 h RAm right ascension J2000 min RAs right ascension J2000 s DE- declination sign --- DEd declination J2000 deg DEm declination J2000 arcmin DEs declination J2000 arcsec RA1950h right ascension B1950.0 h RA1950m right ascension B1950.0 min RA1950s right ascension B1950.0 s DE1950- declination sign --- DE1950d declination B1950.0 deg DE1950m declination B1950.0 arcmin DE1950s declination B1950.0 arcsec S4.83GHz 4.830 GHz Green Bank flux density mJy S/N Signal-to-noise ratio of the detection. The MGIV source list is defined by S/N >= 5 --- G Group containing the source G is defined by the north or south survey detecting the source and the source location in the survey. Sources with b > +10 deg and detected in the south, north, or both surveys are assigned to groups 0, 1, 2. Sources lying in regions observed only once or at low Galactic latitude |b| < 10 deg, and detected in the south, north, or both surveys are assigned to groups 3, 4, or 5. Sources in the region observed twice but with b < -10 deg and detected in south, north, or both surveys, are assigned to groups 6, 7, or 8 --- alpha The NRAO 1400 MHz-MGIV spectral index, alpha(1400 MHz, 4830 MHz), where S {prop.to.} {nu}^alpha^ --- Patricia Bauer, Francois Ochsenbein CDS 1998 Oct 07 Mark Griffith griffith@maggie.mit.edu Authors' addresses: Mark Griffith, Bernard Burke, Sam Conner, And Mike Heflin: Room 26-335, Massachusetts Institute of Technology, Cambridge, MA 02139 (Phone 1-617-253-2572) Glen Langston National Radio Astronomy Observatory , Edgemont Road, Charlottesville, Va 22903 (Phone 1-804-296-0328) UNKNOWN UNKNOWN * 13-Oct-1998: the suffix 'a' or 'b' was added in byte position 14 of table4 to distinguish sources with colliding names. (done for consecutive identical names) * 13-Oct-1998: the suffix 'a' 'b' or 'c' was added in byte position 14 (done for all 132 sources with colliding names) J_ApJS_75_801.xml Photoelectric UBV photometry of stars selected in the HK objective-prism survey J/ApJS/76/1001 J/ApJS/76/1001 UBV photometry of HK survey stars Photoelectric UBV photometry of stars selected in the HK objective-prism survey G W Preston S A Shectman T C Beers Astrophys. J. Suppl. Ser. 76 1001 1991 1991ApJS...76.1001P J/PASP/102/1392 : UBV photometry from HK survey. I (Doinidis+ 1990) J/PASP/103/973 : Photoelectric UBV from HK survey. II (Doidinis+ 1991) J/AJ/108/268 : HK survey emission-line candidates positions (Beers+ 1994) J/AJ/112/1188 : HK survey emission-line candidates (Beers+ 1996) Beer T.C., Preston G.W., and Shectman S.A. =1985AJ.....90.2089B Beer T.C., Preston G.W., and Shectman S.A. =1988ApJS...67..461B Burstein D. and Heiles C., =1982AJ.....87.1165B Photometry, UBV photometry stars: horizontal-branch stars: weak-line Photoelectric UBV observations of 1782 stars are used to explore properties of the HK objective-prism survey conducted by Beers, Preston, and Shectman with the Curtis-Schmidt telescope of the Cerro Tololo Inter-American Observatory. We construct an intrinsic (U-B)0 versus (B-V)0 relation for blue horizontal branch stars and use it to derive estimates of E(B-V) color excesses in 50 survey fields. Comparison of these with the reddening maps of Burstein and Heiles indicates good agreement except in low-latitude fields toward the Galactic bulge. We describe qualitative features of the stellar content of the HK survey by use of unreddened two-color diagrams and indicate how the photometric data may prove useful in several applications. Finally, we use a halo density model to estimate the variation of completeness with apparent magnitude, B, in our catalog of field horizontal branch star candidates.
Data for BHB candidates Data for metal-poor candidates Data for stars with ambiguous HK survey spectral classes Field Curtis-Schmidt field number --- Star Field star number --- m_Star Multiplicative index on star name --- Sp Catalog spectral class --- Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag GLON Galactic longitude deg GLAT Galactic latitude deg Code Code number=1 a: Observed in 1987-1989 at 2.5m telescope by G. Preston b: Observed in 1987-1989 at 1.0m telescope by G. Preston c: Observed prior to 1985 at 1.0m telescope by G. Preston d: Observed prior to 1985 at 1.0m telescope by J.Pier Multiple observations are indicated by digits that follow code letters --- Note Note number=2 1: star was used to derive BHB intrinsic two-color relation 2: star has optical companion within 10" 3: variable? Star seemed too faint at time of observation 4: star is regarded as variable on basis of standard deviations in V and B-V 5: star 12a is NW member of pair, stars 12b is SE member of pair RR: RR Lyrae --- Simona Mei, Patricia Bauer CDS 1995 Jan 30 UNKNOWN UNKNOWN Keypunched at CDS J_ApJS_76_1001.xml Optical spectroscopy of Magellanic Cloud planetary nebulae. II. J/ApJS/76/1085 J/ApJS/76/1085 LMC & SMC PNe optical spectroscopy. II Optical spectroscopy of Magellanic Cloud planetary nebulae. II. S J Meatheringham M A Dopita Astrophys. J. Suppl. Ser. 76 1085 1991 1991ApJS...76.1085M J/MNRAS/234/583 : Abundances in Magellanic Cloud planetary nebulae J/ApJS/75/407 : PNe Magellanic Cloud optical spectroscopy. I J/ApJS/83/87 : PNe Magellanic Cloud optical spectroscopy. III J/A+AS/121/407 : LMC planetary nebulae positions (Leisy+ 1997) Magellanic Clouds Nebulae, planetary Spectroscopy Magellanic Clouds nebulae: planetary We present optical spectroscopy in the range 3300-7400A for a total of 37 planetary nebulae in the LMC and seven in the SMC. Together with the object from the first paper in the series (1991ApJS...75..407M), we now have accurate emission-line intensities down to a few percent of H{beta} for 77 nebulae in the Magellanic Clouds. Agreement with other authors is excellent. Reddening estimates from Balmer line ratios have been determined, and the line intensities have been dereddened accordingly. Nebular [O III] electron temperature and, where measurable, [S II] densities, are derived. [O II] electron densities are recalculated using appropriate electron temperatures. The [S II] and [O II] electron densities correlate well, with n_e_([O II])>n_e_([S II]). Zanstra temperatures are in derived for 22 objects possessing detectable stellar continua. These temperatures are in agreement with photoionization modeling of this sample.
Corrected line intensities Lambda Wavelength 0.1nm ID Identification of wavelength --- PN Plametary nebula name --- I(Lambda) Corrected line intensity (I(Hbeta)=100) --- n_I(Lambda) s: saturated --- Patricia Bauer CDS 1996 Oct 03 Pierre Leisy <leisy@iap.fr> J_ApJS_76_1085.xml A catalog of absorption in the spectra of quasi-stellar objects. J/ApJS/77/203 J/ApJS/77/203 A catalog of absorption in the spectra of quas A catalog of absorption in the spectra of quasi-stellar objects. V Junkkarinen A Hewitt G Burbidge Astrophys. J. Suppl. Ser. 77 203 1991 1991ApJS...77..203J A catalog of absorption in the spectra of quasi-stellar objects. V Junkkarinen A Hewitt G Burbidge Astrophys. J. Suppl, Ser. 81 409 1992 1992ApJS...81,,409J galaxies: distances and redshifts line: identification quasars: general (Abstract of the paper) This paper contains a compilation of basic information on QSO absorption systems. A total of 724 QSOs are listed in three tables. Table 1 contains 353 QSOs that have absorption-line systems with measured redshifts. The numerous Ly{alpha} forest systems based only on narrow hydrogen lines are excluded from Table 1. Absorption systems with multiple components are listed only once in all of the components fall within a span of 500 km/s. A total of 862 systems with narrow metal lines which we consider to be reliably identified are listed in Table 1. Table 1 contains an additional 260 systems consisting of less certain systems, damped Ly{alpha} systems, and Lyman limit systems that have not detected narrow metal lines. In Table 2 we list 146 broad absorption line QSOs. Fifteen of these have narrow absorption line systems identified, and thus they also appear in Table 1. In Table 3 we give an inhomogeneous list of 240 QSOs in which absorption systems have been seen but not measured.
QSO names and positions Coor Coordinate designation 1950 --- RAh1 Right ascension 1950 h RAm1 Right ascension 1950 min RAs1 Right ascension 1950 s DE- Declination sign --- DEd1 Declination 1950 d DEm1 Declination 1950 arcmin DEs1 Declination 1950 arcsec RAh2 Right ascension 2000 h RAm2 Right ascension 2000 min RAs2 Right ascension 2000 s DE- Declination sign --- DEd2 Declination 2000 d DEm2 Declination 2000 arcmin DEs2 Declination 2000 arcsec z(em) Emission redshift --- u_z(em) Uncertainty flag on the emission redshift --- V Apparent magnitude mag n_V A '*' indicates variability --- Jname Coordinate designation J2000 --- name1 Other name --- name2 Other name --- name3 Other name --- name4 Other name -- Com Comments --- QSO absorbing systems Name J name --- Sys Running number for the systems in order of increasing redshift. Where no number appears before an absorption-line system, that system is considered by the authors to be less certain except if BAL (Broad Absorption Line) or possible BAL --- B B= BAL, ? = possible BAL --- z(abs) Absorption redshift or first interval value of z(abs) for BAL or possible BAL --- n_z(abs) A '-' denotes an interval of redshift for BAL or possible BAL --- z(abs)2 Second interval value of z(abs) when n_z(abs)='-' --- N Number which is the multiplicity of redshifts within 500 km/s (in the rest frame) of the values listed --- ref_z(abs) Primary reference used --- Ion1 Ion in absorption --- Ion2 Ion in absorption --- Ion3 Ion in absorption --- Ion4 Ion in absorption --- Ion5 Ion in absorption --- Ion6 Ion in absorption --- Ion7 Ion in absorption --- Ion8 Ion in absorption --- Ion9 Ion in absorption --- Ion10 Ion in absorption --- Ion11 Ion in absorption --- Ion12 Ion in absorption --- Ion13 Ion in absorption --- Ion14 Ion in absorption --- Ion15 Ion in absorption --- Ion16 Ion in absorption --- Ion17 Ion in absorption --- Ion18 Ion in absorption --- Ion19 Ion in absorption --- Ion20 Ion in absorption --- Ion21 Ion in absorption --- ref2 Other reference --- ref3 Other reference --- ref4 Other reference --- ref5 Other reference --- ref6 Other reference --- ref7 Other reference --- Broad Absorption Line QSOs QSOs with absorption lines detected Name Coordinate designation 1950 --- n_Name A "*" indicates that the object also appears in table1 --- name Most frequently used other name --- n_name A "*" indicates a QSO near the listed NGC galaxy with no coordinates given for the QSO. The coordinates of the NGC galaxy are listed (table3) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec V Apparent magnitude mag n_V A '*' indicates variability --- z(em) Emission redshift --- u_z(em) Uncertainty flag on the emission redshift --- Ref References to papers in which absorption was reported. A question mark indicates "possible" BAL --- References in numerical order References in alphabetic order Ref Reference number number= If you decide to copy these files, please send a note with your name and address to Professor G. Burbidge (by e-mail care of B. Travell, address: CASS::TRAVELL_OIR (SPAN type address) or by regular mail to G. Burbidge CASS 0111, UCSD, La Jolla, CA 92093-0111). This will help us judge the usefulness of this electronic distribution and we will use the information to make a mailing list for errata etc. Questions regarding the ftp computer account and any problems with the electronic copies should be addressed to Vesa Junkkarinen (e-mail to: vesa@cass157.ucsd.edu). Please provide the usual acknowledgement/reference to the appropriate Ap. J. Supplement paper if these electronic tables are used in published research. --- dot number= If you decide to copy these files, please send a note with your name and address to Professor G. Burbidge (by e-mail care of B. Travell, address: CASS::TRAVELL_OIR (SPAN type address) or by regular mail to G. Burbidge CASS 0111, UCSD, La Jolla, CA 92093-0111). This will help us judge the usefulness of this electronic distribution and we will use the information to make a mailing list for errata etc. Questions regarding the ftp computer account and any problems with the electronic copies should be addressed to Vesa Junkkarinen (e-mail to: vesa@cass157.ucsd.edu). Please provide the usual acknowledgement/reference to the appropriate Ap. J. Supplement paper if these electronic tables are used in published research. --- Text Reference text number= If you decide to copy these files, please send a note with your name and address to Professor G. Burbidge (by e-mail care of B. Travell, address: CASS::TRAVELL_OIR (SPAN type address) or by regular mail to G. Burbidge CASS 0111, UCSD, La Jolla, CA 92093-0111). This will help us judge the usefulness of this electronic distribution and we will use the information to make a mailing list for errata etc. Questions regarding the ftp computer account and any problems with the electronic copies should be addressed to Vesa Junkkarinen (e-mail to: vesa@cass157.ucsd.edu). Please provide the usual acknowledgement/reference to the appropriate Ap. J. Supplement paper if these electronic tables are used in published research. --- Patricia Bauer CDS 1994 May 27 J_ApJS_77_203.xml Spectroscopy of galaxies in distant clusters. IV. A catalog of photometry and spectroscopy for galaxies in seven clusters with 0.35<z<0.55 J/ApJS/78/1 J/ApJS/78/1 Photometry & Spectroscopy For Galaxies In 7 Clust. Spectroscopy of galaxies in distant clusters. IV. A catalog of photometry and spectroscopy for galaxies in seven clusters with 0.35<z<0.55 A Dressler J E Gunn Astrophys. J. Suppl. Ser. 78 1 1992 1992ApJS...78....1D galaxies: clusters: general galaxies: distances and redshifts *** No Description Available ***
CL0909+4408 DATA r < 22.58 CL0024+1654 DATA r < 22.71 CL0939+4713 DATA r < 22.79 CL0303+1706 DATA r < 22.94 CL 3C295 DATA r < 23.20 CL1601+4253 DATA r < 23.77 CL0016+1609 DATA r < 23.84 N catalog number of each object --- X x coordinate of the object from a central bright galaxy listed in Table 9 of the paper. (aligned to the cardinal directions for all but CL0024+1654, see paper) arcsec Y y coordinate (see above) arcsec rr r magnitude within the fitting radius mag rt total r magnitude * The explanations for columns (4) and (5) in the paper (p47) seem to be different from those in the top of each Table. mag g-r g-r color mag r-i r-i color (for g, r, i color system, see paper) mag TY fitting class for the best fit 'd'=de Vaucouleurs, 'u'=unresolved, 'e'=exponential --- Rf fitting radius arcsec SIZE effective (half-light) radius arcsec rSB r surface brightness (average surface brightness inside the effective radius) * The unit is not described in the paper, and is cited from Schneider et.al. 1986. mag/arcsec2 AXR axial ratio (if significantly determined at greater than the 1 sigma level) --- PA position angle of above deg FLG caution flag for the fit 'A'=asymmetric, 'C'=confused, 'F'=too flat 'S'=sky is more than 5 sigma deviant (see paper in detail) --- SGFLX fractional standard deviation (including only the contribution of pixel variance) of the flux --- SGF sigma corresponding to the goodness of fit for the best-fitting --- SGN above for the next-best fitting --- Z determined redshift --- u_Z uncertainty flag of Z --- SPTYPE alphanumeric code of three letters (separated by commas) giving information about the spectra (see paper, p50) --- QSP quality code (see paper, p50) --- Koichi Nakajima CDS 1993 Dec 02 UNKNOWN UNKNOWN The catalogue was provided by courtesy of A.Dressler to H. Andernach; it was numbered A141 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 16-Apr-1994: First archived. (The date of the latest archiving, see the date of each file.) J_ApJS_78_1.xml A catalog of CO-added IRAS fluxes of Orion population stars J/ApJS/78/239 J/ApJS/78/239 Orion stars CO-added IRAS fluxes catalog A catalog of CO-added IRAS fluxes of Orion population stars W B Weaver G Jones Astrophys. J. Suppl. Ser. 78 239 1992 1992ApJS...78..239W catalogs infrared: stars stars: emission-line, Be stars: pre-main sequence A catalog of co-added IRAS fluxes for the pre-main-sequence objects in the Herbig-Bell catalog (HBC) is presented. This catalog doubles the number of HBC stars with detected IRAS fluxes and provides improved flux values for the previously known sources. Noise levels are given for all HBC fields in each band, permitting upper limits to be estimated for all undetected sources.
Catalog of Coadded IRAS Fluxes of Orion Population Stars HBC Herbig-Bell Catalog Number --- Name Primary name, taken from the HBC number=1 If the name is too long to fit, it is included in the comments or notes. --- e_f12 rms uncertainty on f12 number=2 rms deviation of the residuals after the baseline fit by SCANPI. mJy f12 12 micron flux estimate Jy e_f25 rms uncertainty on f25 number=2 rms deviation of the residuals after the baseline fit by SCANPI. mJy f25 25 micron flux estimate Jy e_f60 rms uncertainty on f60 number=2 rms deviation of the residuals after the baseline fit by SCANPI. mJy f60 60 micron flux estimate Jy e_f100 rms uncertainty on f100 number=2 rms deviation of the residuals after the baseline fit by SCANPI. mJy f100 100 micron flux estimate Jy PSC(f12) 12 micron flux estimate from the IRAS Point Source Catalog (PSC) Jy n_PSC(f12) PSC(f12) note --- PSC(f25) 25 micron PSC estimate Jy n_PSC(f25) PSC(f25) note --- PSC(f60) 60 micron PSC estimate Jy n_PSC(f60) PSC(f60) note --- PSC(f100) 100 micron PSC estimate Jy n_PSC(f100) PSC(f100) note --- IRAS IRAS PSC number --- Qual Quality estimates number=3 a: high quality, est. errors < 10% b: intermediate quality, est. errors 10-25% c: low quality, est. errors > 25% or minimum detection x: no signal detected y: no measurement possible, usually because of a strong, nearby source --- Notes Processing notes number=4 dxx: deconvolution was performed at xx microns exx: extended source detected of xx width (arcmin) (): offset in arcmin, positive in northerly direction *: object has comments in table5.dat For example, HBC 17 lists d12e2.5(-0.7) as the first part of the processing notes. This means that the default 12 micron flux was changed after it was examined with DECON, a deconvolution program described in the published paper. The point response function of the IRAS beam was convoluted with a rectangular source of 2.5arcmin full width to provide the best fit to the scan. The resulting integrated flux was 24.00Jy (fourth data field) and this extended source was offset 0.7arcmin in a southerly direction with respect to the HBC coordinates. --- Notes to table 4 HBC Herbig-Bell Catalog Number, if blank, the text continues the previous record --- Name Text of the note --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 26-Oct-1994 May 11 Addresses: Weaver W.B. and Jones G. Monterey Institute for Research in Astronomy, 900 Major Sherman Lane, Monterey, CA 93940 AAS CD-ROM series, Volume 2, 1994 J_ApJS_78_239.xml The Bell Laboratories H I Survey - High Velocity Cloud Catalog J/ApJS/79/77 J/ApJS/79/77 Bell Lab. H I Survey - High Velocity Clouds The Bell Laboratories H I Survey - High Velocity Cloud Catalog A A Stark C F Gammie R W Wilson J Bally R A Linke Astrophys. J. Suppl. 79 77 1992 1992ApJS...79...77S H I data Interstellar medium Radio sources Surveys The sky north of declination -40 deg. was observed in the 21 cm line of atomic hydrogen with the FWHM = 2 deg. beam of the 20 foot horn reflector at AT&T Bell Laboratories, Crawford Hill. The survey covers a velocity range of 654 km/s centered on the Galactic standard of rest, with 5.3 km/s wide filters. This survey is distinguished by its sensitivity to low surface brightness features (antenna temperature about 50 mK) and relative freedom from sidelobe contamination. The high-velocity cloud list was extracted and cataloged automatically from the survey data.
Observations were made as drift scans along even declinations between -40 deg. and +90 deg. at the epoch (1981) of the observations. The horn antenna has a FWHM beam size of 2 deg. at 21 cm. The average rms noise of spectra taken at all declinations is 0.017 K in 5.2 km/s wide channels, although in some cases naseline problems make the survey unreliable at this level. The clouds cataloged were selected to be those near for which the velocities, when projected on the galactic plane at each possible distance, differed from the circular rotation velocities by more than 40 km/sec. The boundaries of the clouds were determined by either a decrease in emission to near the baseline emission or a steep drop in antenna temperature.
The catalog of high-velocity clouds num [1,1313] Running number --- pkRAdeg Right Ascension (1950) of peak emission deg pkDEdeg Declination (1950) of peak emission deg pkGLON Galactic longitude of peak emission deg pkGLAT Galactic latitude of peak emission deg maxGLON Maximum galactic longitude of cloud deg minGLON Minimum galactic longitude of cloud deg maxGLAT Maximum galactic latitude of cloud deg minGLAT Minimum galactic latitude of cloud deg maxvel Maximum velocity of cloud km/sec minvel Minimum velocity of cloud km/sec flux Total flux K.km/sec antemp Peak antenna temperature K o_cl Number of points cloud detected --- N.G. Roman NASA/NSSDC/ADC 1994 Aug 10 J_ApJS_79_77.xml The structure of southern extragalactic radio sources. J/ApJS/80/137 J/ApJS/80/137 Southern Extragalactic Radio Sources The structure of southern extragalactic radio sources. P A Jones W B McAdam Astrophys. J. Suppl. Ser. 80 137 1992 1992ApJS...80..137J Galaxies, radio Radio sources Surveys galaxies: distances and redshifts galaxies: photometry radio continuum: galaxies surveys techniques: interferometric This catalog contains a list of 384 extragalactic radio sources south of declination -30{deg} which have been imaged with the Molonglo Observatory Synthesis Telescope (MOST) at 843 MHz with a HPBW of 44" x 44" cosec(dec). The sample includes those sources noted in the Molonglo Reference Catalog (MRC) (Cat.<VIII/16>) as extended (larger than 1'), as well as those noted as multiple (within 8' of another ssource and possibly related). The sample is representative of the strong extended extragalactic radio sources of the southern sky, but is not statistically complete. Positions, flux densities, and sizes are given for all sources, and those sources which have been confirmed as extended MRC sources are flagged. In addition, optical positions, magnitudes, redshifts, and identifications are given for 201 of the sources. These data were originally published in two tables which have been merged in this version.
Structure of Southern Extended Extragalactic Radio Sources Cflag Confirmation Flag for MRC Extended Source Sample number=1 This column is marked with a 'C' if the source is a member of the Confirmed MRC Extended Sample. Sources in this study were selected from the MRC if they were extended, slightly extended, complex, or multiple sources. Those sources which have angular size larger than 0.5' and flux density greater than 0.4 Jy at 843 MHz are considered confirmed as extended radio sources. The confirmed sample is not complete to the limits of these criteria, however, because the flagging procedures in the MRC (Large et al. 1981MNRAS.194..693L) were conservative. --- Name Name of source, followed by source flags number=2 This column gives the name of the source, comprised of the hours and minutes of right ascension, the sign of the declination, the degrees, to the nearest tenth of a degree. In addition, a capital letter is appended to the name to distinguish components. The following source flags may also be appended to the source name: * Single source which has multiple listings in the MRC. c Two or three sources that are combined in one MRC listing. N Nearby source, listed in MRC but not flagged. n Nearby source, not listed in MRC. --- f_Name Source flag number=2 This column gives the name of the source, comprised of the hours and minutes of right ascension, the sign of the declination, the degrees, to the nearest tenth of a degree. In addition, a capital letter is appended to the name to distinguish components. The following source flags may also be appended to the source name: * Single source which has multiple listings in the MRC. c Two or three sources that are combined in one MRC listing. N Nearby source, listed in MRC but not flagged. n Nearby source, not listed in MRC. --- S843 Integrated flux density at 843 MHz, in Jy number=3 This column gives the integrated flux density of the source at 843 MHz, in Jy. The integrated flux densities have an rms uncertainty of +/- 9%, of which 6% arises from the calibration of the observations and 7% from the integration. The results were checked against previously published data, and systematic errors were estimated to be less than 5% in flux density (including uncertainty in the absolute flux density scale). Jy RAh Right Ascension (B1950) (hour) number=4 These columns give the B1950 right ascension and declination of the centroid position. These positions have an accuracy of 1.6" in right ascension and 2.2" cosec(dec) in declination. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=4 These columns give the B1950 right ascension and declination of the centroid position. These positions have an accuracy of 1.6" in right ascension and 2.2" cosec(dec) in declination. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec f_Size Size flag for the source number=5 These columns give the size flag, angular size (in arcmin) and position angle (in degrees) of the source. The angular size is to be understood according to the size flag as follows: d Separation of peaks in a double source. e Largest separation of peaks in a complex source. l Largest size of low-brightness emission in a complex sources. m Deconvolved extent along axis of source. s Largest separation of centroids of nearby sources. In this case, the size is the distance between components which may be matched by examination of the source names. The position angle (north through east) of the peak separation or deconvolved major axis is given except for a few curved sources where the quoted position angle refers to the axis of the central region. --- Size Angular size of the source number=5 These columns give the size flag, angular size (in arcmin) and position angle (in degrees) of the source. The angular size is to be understood according to the size flag as follows: d Separation of peaks in a double source. e Largest separation of peaks in a complex source. l Largest size of low-brightness emission in a complex sources. m Deconvolved extent along axis of source. s Largest separation of centroids of nearby sources. In this case, the size is the distance between components which may be matched by examination of the source names. The position angle (north through east) of the peak separation or deconvolved major axis is given except for a few curved sources where the quoted position angle refers to the axis of the central region. arcmin PA Position angle of source number=5 These columns give the size flag, angular size (in arcmin) and position angle (in degrees) of the source. The angular size is to be understood according to the size flag as follows: d Separation of peaks in a double source. e Largest separation of peaks in a complex source. l Largest size of low-brightness emission in a complex sources. m Deconvolved extent along axis of source. s Largest separation of centroids of nearby sources. In this case, the size is the distance between components which may be matched by examination of the source names. The position angle (north through east) of the peak separation or deconvolved major axis is given except for a few curved sources where the quoted position angle refers to the axis of the central region. deg nearflg '*' if nearby source and flux is combined number=6 This column is flagged with an asterisk ('*') if there is a nearby source to which the angular size refers. In these cases, the size was often listed for multiple components in the published version, grouped together with brackets. Pairs of sources were also sometimes given angular sizes for both the separation of centroids and the separation of peaks in a double. Components may be matched by examination of the source names. --- newflg 'n' if optical info is new identification number=7 This column is flagged with an 'n' if the optical identification is new in this survey. --- RAoh Right Ascension (B1950) (hour) number=8 These columns give the B1950 optical right ascension and declination of the source. Film copies of the UK Schmidt IIIaJ survey were searched for optical identifications. Optical positions were measured with a two-coordinate measuring machine, using nearby reference stars from the SAO and Cape star catalogs (Hunstead 1971MNRAS.152..277H). The plate parameters were determined by a least-squares six-parameter fit to the reference stars to give optical positions with an estimated accuracy of 0.5" in each coordinate. h RAom Right Ascension (B1950) (min) min RAos Right Ascension (B1950) (sec) s DEo- Declination sign (B1950) number=8 These columns give the B1950 optical right ascension and declination of the source. Film copies of the UK Schmidt IIIaJ survey were searched for optical identifications. Optical positions were measured with a two-coordinate measuring machine, using nearby reference stars from the SAO and Cape star catalogs (Hunstead 1971MNRAS.152..277H). The plate parameters were determined by a least-squares six-parameter fit to the reference stars to give optical positions with an estimated accuracy of 0.5" in each coordinate. --- DEod Declination (B1950) (deg) deg DEom Declination (B1950) (arcmin) arcmin DEos Declination (B1950) (arcsec) arcsec Bmag Magnitude of source number=9 The mag column gives the magnitude (b_J_) of the possible optical identifications, estimated to the nearest 0.5 magnitude by comparison of Polaroid enlargements of the Schmidt prints with reference images of galaxies and stars of known magnitude. The reference galaxies were from the lists of Carter (1980MNRAS.190..307C) and Dickens, Currie, and Lucey (1986MNRAS.220..679D), while the stars were from Hawkins (1979, 1981MNRAS.194.1013H). The reference magnitudes were corrected to the survey color using the equation b_J_ = B - 0.23(B - V) (Shanks et al., 1984MNRAS.206..767S). For unresolved radio sources, the search radius for galaxies and stellar objects was 5.6", which is approximately twice the combined radio and optical position errors. mag ID Optical identification of source number=10 Optical identifications are given in the 'ID' column. Galaxies were accepted as identifications of the extended radio sources if the projected optical-radio centroid offsets were less than 50 kpc. The distance was estimated by assuming an absolute magnitude M of -21.0 and making corrections to the apparent magnitude for absorption and redshift. If more than one galaxy satisfied the 50 kpc criterion, the brightest galaxy was chosen. A few identifications were accepted for sources having offsets greater than 50 kpc when there was other evidence supporting the identification (for example, a radio core coincident with the optical object). The following symbols are used: st Stellar image, probably a QSO Q Confirmed QSO BL Confirmed BL Lac object. db Double galaxy (see mult_flg below) --- z Redshift of source number=11 The redshift is given in the z column. Fourteen new redshifts were measured using the Anglo-Australian Telescope. These redshifts are flagged with an 'n' in the f_z column. All known redshifts are listed, for completeness. Redshifts have been obtained from the literature, largely from the compilations of Veron-Cetty and Veron (1983A&AS...53..219V) and Palumbo, Tanzella-Nitti, and Vettolani (1983). The original references are quoted except for three objects with many redshift measurements where the weighted average from Palumbo et al. (1983) was used. ** The redshifts have not been corrected for Galactic rotation. --- f_z 'n' if redshift is new number=11 The redshift is given in the z column. Fourteen new redshifts were measured using the Anglo-Australian Telescope. These redshifts are flagged with an 'n' in the f_z column. All known redshifts are listed, for completeness. Redshifts have been obtained from the literature, largely from the compilations of Veron-Cetty and Veron (1983A&AS...53..219V) and Palumbo, Tanzella-Nitti, and Vettolani (1983). The original references are quoted except for three objects with many redshift measurements where the weighted average from Palumbo et al. (1983) was used. ** The redshifts have not been corrected for Galactic rotation. --- mult_flg '*' if position of another companion is listed below number=12 This column is flagged with an asterisk '*' if the optical identification is a double galaxy and both positions were listed in the published paper. The following second components were given in the published paper: 0618-371 06 18 17.87 -37 10 18.7 0651-603 06 51 16.09 -60 18 28.9 1302-325 13 02 13.07 -32 33 13.4 2130-538 21 30 49.18 -53 51 33.6 2243-529 22 43 13.16 -52 59 17.0 --- Patricio Ortiz CDS 1999 Apr 06 UNKNOWN UNKNOWN "The catalogue was originally archived as A041 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_ApJS_80_137.xml Compact Radio Sources near the Galactic Plane J/ApJS/80/211 J/ApJS/80/211 Compact Radio Sources Near the Galactic Plane Compact Radio Sources near the Galactic Plane D J Helfand S Zoonematkermani R H Becker R L White Astrophys. J. Suppl. 80 211 1992 1992ApJS...80..211H Galactic plane H II regions Milky Way Planetary nebulae Radio sources HII regions nebulae: general radio continuum: galaxies surveys This catalog tabulates the results of the extension of the 20cm Galactic plane survey reported by Zoonematkermani and coworkers to Galactic latitudes of +-1.8 deg over the central region of the Milky Way (-10 deg <= l <= 40 deg). catalog 1457 new discrete radio sources down to flux densities of <=5 mJy an are 95% complete at 20 mJy. A detailed comparison of all radio sources from our complete survey in this longitude range with the IRAS Point Source Catalog proves classification for 13% of the objects, including 159 compact HII regions, and nearly 100 planetary nebulae over 70 of which are newly identified. We comment briefly on the identity of the remaining radio sources and on the importance of our 6cm survey, currently underway, in defining the radio source population of the Galaxy.
compact radio sources near Galactic plane NAME IAUname in format lll.lll+b.bbb --- RAh Right ascension (B1950) h RAm Right ascension (minutes) min RAs Right ascension (seconds) s DE- Declination sign (B1950) --- DEd Declination (B1950)(degrees) deg DEm Declination (minutes) arcmin DEs Declination (seconds) arcsec Speak peak 1490 MHz flux The values of Speak and Sint have been corrected forr the loss of sensitivity of the primary beam of the antennas away from the field centre. mJy Sint integrated 1490 MHz flux mJy diam source diameter The quoted diameters are the mean of the best-fit FWHM of the major and minor axes of the sources as determined by the Gaussian fits. Values of '0.0' were replaced by blank entries at CDS. arcsec offset off-axis angle (for sensitivity correction) arcmin NOTE notes Unfortunately the published notes were not provided with the electronic version. --- Heinz Andernach CDS modified by James E. Gass SSDOO/ADC 1998 Oct 28 UNKNOWN UNKNOWN The files were provided courtesy R.H. Becker to H. Andernach. It was numbered R105 in H.A.'s "List of Astronomical Catalogues and Documents not available from NASA-ADC but kindly provided on request by various authors". The electronic version contained 28 more sources (1485) than the published one (1457), but did not contain the comment column. J_ApJS_80_211.xml Nearby galaxy flows modeled by the light distribution: distances, model, and the local velocity anomaly. J/ApJS/80/479 J/ApJS/80/479 Nearby galaxy flows Nearby galaxy flows modeled by the light distribution: distances, model, and the local velocity anomaly. R B Tully E J Shaya M J Pierce Astrophys. J. Suppl. Ser. 80 479 1992 1992ApJS...80..479T VII/145 : Nearby Galaxies Catalogue (NBG) Pierce M.J. & Tully R.B. 1988, ApJ, 330, 579 =1988ApJ...330..579P Tully R.B. 1987, ApJ, 321, 280 =1987ApJ...321..280T Tully R.B., 1988a, Nearby Galaxies Catalogue (NBG) =Catalogue <VII/145> Tully R.B. 1988c, AJ, 96, 73 =1988AJ.....96...73T Clusters, galaxy Redshifts cosmology: observations galaxies: clusters: general galaxies: distances and redshifts Supporting material for an article in the main journal is presented. One table gives measured galaxy distances used to construct a map of observed peculiar velocities, and another table gives a grid of the distribution of light used to construct a map of expected peculiar velocities. A preferred model was developed which gave a best fit between these maps, and this model has been used to generate output kinematic distances which are recorded here for groups and individual galaxies with V_0_<3000km/s.
Galaxies with distance estimates Group Group identification number=1 Identification in NBG catalog. If more than one galaxy in a group provides a distance estimate then galaxies are identified on subsequent lines. The correspondance between the first number and the galaxy group name are in note file --- Gal Galaxy identification number=2 Galaxies with measured distances, as named in NBG catalog. N=NGC; U=UGC. Virgo, Ursa Major, and Fornax clusters are identified. Galaxies with distances in the Virgo and Ursa Major clusters are identified in Pierce & Tully 1988 --- Memb Group members number=3 Number of galaxies in group, as compiled in NBG catalog. For single galaxies, there is a "1" in this column. Group properties are summarized in Tully 1987. --- Ngal Number of total galaxies --- Ngal2 Number of galaxies with distance estimates when this number is different of Ngal number=4 Up to four separate estimates per galaxy are possible, as explained in text. In the case of groups with multiple estimates, then Ngal/Ngal2 means there are Ngal2 separate galaxies with distance estimates and Ngal total estimates --- Dist Distance number=5 In the case of groups with estimates to several members, the average distance is given on the first line and the individual distance estimates (but averaged over the separate bands) are given on subsequent lines. Position in supergalactic coordinates can be determined by multiplying the value in NBG catalog by the ratio of this distance and the NBG catalog distance. Mpc Vel Velocity number=6 Velocity adjusted to the standard Local Group rest frame (300km/s toward l=90, b=0) and averaged over the number of galaxies indicated in col.(3). See Tully 1987. km/s note Note number=7 The symbol "#" indicates one of 14 cases of poor agreement between measured and kinematic distances. Disregarded in some fits as discussed in text. --- Components of the mass model Group Identification in NBG catalog number=1 The correspondance between the first number and the galaxy group name are in note file. --- Memb Number of galaxies in group number=2 Number of galaxies in group, as compiled in NBG catalog. Includes galaxies directly "associated" with group. Individual galaxies outside of groups are identified by name. --- log(L) Luminosity number=3 Blue band, corrected for absorption and incompletion as a function of distance as described in Tully (1988c) solLum SGX Supergalactic X coordinate Mpc SGY Supergalactic Y coordinate Mpc SGZ Supergalactic Z coordinate Mpc IDist Input distance (vector sum of cols [4]-[6]) of element in light distribution map Mpc ODist Derived distance from velocity field of preferred model number=4 58 cases (out of 776) are resolved in 22 cases by taking the kinematic distance nearest the luminosity-line width distance and resolved in 36 cases without measured distances by taking the kinematic distance nearest to the input distance. (In the 22 cases with independent distance estimates, only four choices differ) Mpc Marie-Jose Wagner, Patricia Bauer CDS 1996 Apr 17 UNKNOWN UNKNOWN Keypunched at CDS J_ApJS_80_479.xml A 20 centimeter VLA survey of Abell clusters of galaxies. II. Images and optical identifications J/ApJS/80/501 J/ApJS/80/501 VLA survey of Abell clusters. II. A 20 centimeter VLA survey of Abell clusters of galaxies. II. Images and optical identifications F N Owen R A White J O Burns Astrophys. J. Suppl. Ser. 80 501 1992 1992ApJS...80..501O VIII/29 : 1400-MHz Survey of 1478 Abell Galaxy Clusters (Owen+ 1982) J/AJ/109/14 : Optical spectroscopy of Abell clusters. I. (Owen+ 1995) J/AJ/109/853 : VLA survey of Abell clusters. IV. (Ledlow+ 1995) J/AJ/110/1959 : VLA survey of Abell clusters. V. (Ledlow+ 1995) Zhao et al., Paper I. 1989AJ.....98...64Z Owen et al., Paper III. 1993ApJS...87..135O Ledlow et al., Paper IV. 1995AJ....109..853L, Cat. <J/AJ/109/853> Ledlow et al., Paper V. 1995AJ....110.1959L, Cat. <J/AJ/110/1959> Owen et al., Paper VII. 1997ApJS..108...41O Clusters, galaxy Radio sources galaxies: active galaxies: clusters: general galaxies: jets radio continuum: galaxies surveys We present radio contour maps, models, and optical identifications for 130 radio galaxies in Abell clusters of galaxies.
Radio galaxy parameters Abell Abell cluster number number=1 1927-A : alternative identification is 14" SE of galaxy marked. 2306-A : Galaxy is at plate limit and does not reproduce well in the glossy. --- --- --- m_Abell Multiplicity index on Abell number --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Rmag Estimate of the R magnitude of the galaxy mag Flux Total flux density of the associated radio source number=2 If the column is blank, the galaxy listed is an alternate identification for the last radio source with a flux density listed about it. mJy MajAxis Major axis of the CLEAN beam of the radio image used for the analysis arcsec MinAxis Minor axis of the CLEAN beam of the radio image used for the analysis arcsec PA Position angle of the CLEAN beam of the radio image used for the analysis deg Ref References number=3 References 1: O'Donoghue A.A., Owen F.N., Eilek J.A., 1990ApJS...72...75O 2: Giovannini G., Feretti L., Gregorini L., 1987A&AS...69..171G 3: Gregorini L., Bondi M., 1989A&A...225..333G 4: Taylor et al., 1990ApJ...360...41T 5: de Ruiter et al., 1986A&AS...65..111D 6: Fanti et al., 1987A&AS...69...57F 7: Zhao J.-H., Burns J.O., Owen F.N., 1989AJ.....98...64Z --- James Marcout, Patricia Bauer CDS 1997 Sep 15 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_80_501.xml An X-ray catalog and atlas of galaxies. J/ApJS/80/531 J/ApJS/80/531 An X-ray catalog and atlas of galaxies. An X-ray catalog and atlas of galaxies. G Fabbiano D -W Kim G Trinchieri Astrophys. J. Suppl. Ser. 80 531 1992 1992ApJS...80..531F Galaxy catalogs X-ray sources atlases catalogs Galaxy: structure X-rays: galaxies An X-ray catalog and atlas of galaxies observed with the Einstein Observatory imaging instruments (IPC and HRI) are presented. The catalog comprises 493 galaxies, including targets of pointed observations, and RSA or RC2 galaxies serendipitously included in Einstein fields. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 2123 sigma upper limits. The other galaxies were either at the edge of the visible field of view or confused with other X-ray sources. For these a rough measure of their X-ray emission is also given. The atlas shows X-ray contour maps of detected galaxies superposed on optical photographs and gives azimuthally averaged surface brightness profiles of galaxies detected with a high signal-to-noise ratio.
Einstein
Observation Info for the EINSTEIN Galaxy Catalog Name Name of the object (NGC, IC, UGC number) --- note Note: 'a' if AGN or 'b' if Virgo --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec nH Foreground column of HI number=1 This column contains the Galactic column density of HI in the direction of the galaxy in question, in units of 10^20^ cm^-2^. The information is accurate to two significant digits. 10+20cm-2 inst Instrument used number=2 instrument flag (I for IPC, and H for HRI), and the sequence number of the observation. --- Seqno Observation sequence number --- obs.Y Year of start of observation minus 1900 yr obs.D Day of start of observation d livetime Time of observation number=3 This column contains the total livetime of the observing sequence in seconds, quoted to one decimal place. s offaxis Distance to field center number=4 This column gives the angular separation between the center of the field for the observing sequence and the optical position of the galaxy. It is given in arcminutes, to an accuracy of 0.1 arcminute. arcmin Flux Density Info for the EINSTEIN Galaxy Catalog Name Name of the object (NGC, IC, UGC number) --- note Flag indicating ending note number=1 This column gives a flag if there is a note on the source. The following are used: `a' if the galaxy has an AGN `b' if it is a Virgo cluster member `c' X-ray data are from the following: LMC and SMC: Long and van Speybroeck (1983) in "Accretion Driven X-Ray Sources" Lewin and van den Heuvel eds. (Cambridge: Cambridge U. Press) p. 117. M31 and M32: Trinchieri and Fabbiano (1991ApJ...382...82T) M33: Trinchieri et al. (1988ApJ...325..531T) M101: Trinchieri et al. (1990ApJ...356..110T) `d' no morphological type available (peculiar galaxy) `e' combined flux of two sources (see table 7 of published paper) --- RAh Right Ascension (B1950) (hour) h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec instr Instrument used number=2 I for IPC, and H for HRI --- seqno Observation sequence number number=3 A sequence number of 99999 indicates that there is more than one observation of the source. See the gxatlas.dat table for details on the observations. --- Bmag Apparent B magnitude number=4 This column gives the B-band apparent magnitude from the RSA, RC2 or PCG (Patural's Principal Catalog of Galaxies). (Cat. <VII/119>) mag type T-type following RC2 number=5 This column gives the T-type, as defined in the RC2 (Cat. <VII/112>), using morphological information from the RSA, RC2, or PCG. --- RA_Xh Right Ascension (B1950) (hour) number=6 These columns give the B1950 right ascension and declination of the X-ray centroids of those objects detected by EINSTEIN. h RA_Xm Right Ascension (B1950) (min) min RA_Xs Right Ascension (B1950) (sec) s DE_X- Declination sign (B1950) number=6 These columns give the B1950 right ascension and declination of the X-ray centroids of those objects detected by EINSTEIN. --- DE_Xd Declination (B1950) (deg) deg DE_Xm Declination (B1950) (arcmin) arcmin DE_Xs Declination (B1950) (arcsec) arcsec radius Size of aperture for flux extraction arcsec l_counts Flagged '<' if counts is an upper limit number=7 These columns give the total (background-subtracted) X-ray counts or upper limits for all galaxies in the catalog. The error in the counts (1-sigma) is also given for all detected galaxies. A "<" in the l_counts column indicates an upper limit. No error is given for upper limits. --- counts Total counts from EINSTEIN observation number=7 These columns give the total (background-subtracted) X-ray counts or upper limits for all galaxies in the catalog. The error in the counts (1-sigma) is also given for all detected galaxies. A "<" in the l_counts column indicates an upper limit. No error is given for upper limits. ct e_counts Error on count total number=7 These columns give the total (background-subtracted) X-ray counts or upper limits for all galaxies in the catalog. The error in the counts (1-sigma) is also given for all detected galaxies. A "<" in the l_counts column indicates an upper limit. No error is given for upper limits. ct l_crate '<' if count rate is upper limit number=8 The crate column gives the EINSTEIN X-ray count-rate per 1000 seconds. The l_crate column is flagged with a "<" if the count-rate is an upper limit. --- crate Count-rate from EINSTEIN observation number=8 The crate column gives the EINSTEIN X-ray count-rate per 1000 seconds. The l_crate column is flagged with a "<" if the count-rate is an upper limit. ct/ks l_FluxX '<' if flux is an upper limit number=9 The FluxX column gives the EINSTEIN X-ray flux in units of 10E-13 erg/sec/cm2. The l_FluxX column is flagged with a "<" if FluxX is an upper limit. --- FluxX X-ray flux number=9 The FluxX column gives the EINSTEIN X-ray flux in units of 10E-13 erg/sec/cm2. The l_FluxX column is flagged with a "<" if FluxX is an upper limit. 10-16W/m2 dist Assumed distance in Megaparsecs number=10 This column gives the assumed distance in Mpc for all galaxies in the catalog, derived assuming a Hubble constant of 50 km/s/Mpc corrected for Virgocentric inflow. Mpc l_logLx '<' if luminosity is upper limit number=11 The logLx column gives the log of the derived X-ray luminosity (or upper-limit thereof) for all galaxies in the catalog, using the distances given in the distance column. Units are log(ergs/sec). The l_logLx column is flagged with a "<" if logLx is an upper limit. --- logLx Log of the X-ray luminosity number=11 The logLx column gives the log of the derived X-ray luminosity (or upper-limit thereof) for all galaxies in the catalog, using the distances given in the distance column. Units are log(ergs/sec). The l_logLx column is flagged with a "<" if logLx is an upper limit. [10-7W] Patricio Ortiz CDS 1999 Apr 06 UNKNOWN UNKNOWN Prepared from the tables available at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) J_ApJS_80_531.xml Compendium of Radio Spectra and Luminosities for three complete samples of Radio Sources J/ApJS/81/83 J/ApJS/81/83 Compendium of Radio Spectra and Luminosities Compendium of Radio Spectra and Luminosities for three complete samples of Radio Sources T Herbig A C S Readhead Astrophys. J. Suppl. 81 83 1992 1992ApJS...81...83H Radio sources Redshifts This catalog is a complete sample of 256 powerful extragalactic radio sources. The catalog includes source idenfification, redshift, luminosities and spectral indices at standard rest frequencies as well as bolometric luminosities between emitted frequencies of 10 MHz and 100 GHz. The paper also includes fits to the measured radio spectra which have not been included in this catalog.
Table 1 of Herbig & Readhead 1992, ApJS 81, 83 IAUname IAU name of the object. --- name Other common name. --- z Redshift of the object. --- n_z [* ] * means Estimated redshifts For 18 of the sources no redshifts were available. For Sources with optical identifications but no reliable published redshifts, these were estimated from their apparent optical magnitudes. In the case of five sources not identified optically, a redshift of 1 was assumed. The redshift of these sources has been flagged with a * in this field. --- P_150 Emitted Luminosity at 150 MHz Emitted specific luminosities at the emitted frequencies shown for a value of the Hubble constant of Ho = 100 h km/s/Mpc. The values scale with (H/Ho)^-2. To estimate the fluxdensities measured data points were interpolated with a cubic spline fit to the observed flux densities. Most fits were made in the log S(nu) - log (nu) plane. Closeness of the spline fit was adjusted by eye with the parameter phi. Specific luminosities were evaluated at the satndard frequencies for a universe with qo=0.5 and Lambda=0. The bolometric luminosities were calculated from the spline fits. To extrapolate to the limits of the band the spectra were extended as power laws from the endpoints of the spline fits. W/Hz P_2500 Emitted Luminosity at 2.5 GHz W/Hz P_4000 Emitted Luminosity at 40 GHz W/Hz Pbol Emitted bolometric luminosities W alph150 Spectral index (S ~ nu^alpha at 150MHz) --- alph2500 Spectral index at 2.5 GHz --- alph4000 Spectral index at 40 GHz --- phi Spline fitting parameter --- mem [ABC ] Sample membership (A) revised 3CR survey of Laing et al. 1983 (LRL) (B) survey of Peacock and Wall 1981 (PW) (C) VLBI sample of Pearson and Readhead 1988 (PR). --- r_z References to redshifts (1) Laing et al. 1983 (2) Pearson and Readhead 1988 (3) Peacock and Wall 1981 (4) Riley, priv. comm. (5) Lawrence, priv. comm. (6) Xu, priv. comm. (7) Murphy 1988 (8) Veron and Veron 1981 (9) Spencer et al. 1989 (10) Hewitt and Burbidge 1987. A blank in this column indicates that no reliable redshift is available. The sources designated as "U" are not identified optically. --- N.P.M. Kuin ADC/SSDOO/NASA 1995 Feb 14 J_ApJS_81_83.xml A homogeneous catalog of new UBV and H-beta photometry of B and A type stars in and around the Scorpius-Centaurus OB association J/ApJS/82/117 J/ApJS/82/117 UBV and H-beta in Sco-Cen association A homogeneous catalog of new UBV and H-beta photometry of B and A type stars in and around the Scorpius-Centaurus OB association R W Slawson R J Hill J D Landstreet Astrophys. J. Suppl. Ser. 82 117 1992 1992ApJS...82..117S Photometry, H-beta Photometry, UBV Stars, early-type open clusters and associations: individual (Sco-Cen association) stars: early-type stars: fundamental parameters As part of a thorough study of the luminosity function of Sco-Cen, UBV, and H_{beta}_ photometry has been acquired for a large number of mid B- to late A-type stars which are within or surrounding the Scorpius-Centaurus OB association. UBV and H_{beta}_ photoelectric measures have been obtained for all the B stars without previous observations and for many of those with in the large field 280deg<=l<=362deg, +10deg<=b<=+40deg, and m-M<=7.5mag. Within the upper Scopius subgroup (ScoOB2), 341deg<=l<=362deg, +10=<b=<30deg, UBV and H_{beta}_ photometry was obtained for all B stars listed in the MSC(HD) catalog. As well, UBV measures were obtained for all the A-type stars within this field.
Mean UBV observations Name HD, CD or CPD number --- Vmag V magnitude mag e_Vmag rms uncertainty in Vmag mag n_Vmag Note on Vmag number=1 An asterisk after an uncertainty value for a V, B-V, or U-B magnitude indicates probable variability based on a chi-squared test. --- B-V B-V colour mag e_B-V rms uncertainty in B-V mag o_Vmag Number of observations contributing to B and V --- n_B-V Note on B-V number=1 An asterisk after an uncertainty value for a V, B-V, or U-B magnitude indicates probable variability based on a chi-squared test. --- U-B U-B magnitude mag e_U-B rms uncertainty in U-B mag o_U-B Number of observations in U filter --- n_U-B Note on U-B number=1 An asterisk after an uncertainty value for a V, B-V, or U-B magnitude indicates probable variability based on a chi-squared test. --- Mean H-beta observations HD HD Number --- m_HD Multiplicity index on HD --- Hbeta H-beta index --- e_Hbeta rms uncertainty in H-beta --- o_Hbeta Number of individual observations --- n_Hbeta Note on Hbeta number=1 An asterisk after the uncertainty in the H-beta index indicates probable variability based on a chi-squared test. --- table4.tex Plain TeX version of table4 table5.tex Plain TeX version of table5 Francois Ochsenbein CDS 1995 Feb 16 Bob Slawson, The Univ. of Western Ontario <bslawson@phobos.astro.uwo.ca> J_ApJS_82_117.xml Observations of double stars and new pairs. XV. J/ApJS/83/351 J/ApJS/83/351 Observations of double stars and new pairs. XV. Observations of double stars and new pairs. XV. W D Heintz Astrophys. J. Suppl. Ser. 83 351 1992 1992ApJS...83..351H binaries: visual *** No Description Available ***
New pairs Name Hei denomination --- RAh Right ascension 1900 h RAm Right ascension 1900 min RAs Right ascension 1900 s DE- Declinaiton sign --- DEd Declination 1900 deg DEm Declination 1900 arcmin DEs Declination 1900 arcsec BD/CPD BD or CPD name --- Observations with 61 cm refractor Observations with the Cerro Tololo reflectors Name Name --- RAh Right ascension 2000 h RAdm Right ascension 2000 (deci-minutes) 0.1min DE- Declination sign --- DEd Declination 2000 deg DEm Declination 2000 arcmin Obs Observation date yr PA Position angle deg u_PA uncertainty flag on PA s for single, r for round (single star seen) --- Sep Separation angle deg u_Sep uncertainty flag on Sep --- n Number of nights of observations --- Tel Telescope designation as Y = 1m Yale reflector L = 0.60m Lowell reflector blank = 0.91m Tololo reflector --- Comp Components for multiple systems --- m1 Magnitude of brightest component mag dash Separator --- m1 Magnitude of brightest component mag Patricia Bauer CDS 1994 Jun 27 J_ApJS_83_351.xml Optical spectroscopy of Magellanic Cloud planetary nebulae. III. J/ApJS/83/87 J/ApJS/83/87 LMC & SMC PNe optical spectroscopy. III Optical spectroscopy of Magellanic Cloud planetary nebulae. III. E Vassiliadis M A Dopita D H Morgan J F Bell Astrophys. J. Suppl. Ser. 83 87 1992 1992ApJS...83...87V J/MNRAS/234/583 : Abundances in Magellanic Cloud planetary nebulae J/ApJS/75/407 : PNe Magellanic Cloud optical spectroscopy. I J/ApJS/76/1085 : PNe Magellanic Cloud optical spectroscopy. II J/A+AS/121/407 : LMC planetary nebulae positions (Leisy+ 1997) Magellanic Clouds Nebulae, planetary Spectroscopy Magellanic Clouds nebulae: planetary We present optical spectroscopy in the range 3300-7400A for a total of 52 planetary nebulae in the Large Magellanic Cloud (LMC) and 18 in the Small Magellanic Cloud (SMC). Together with the object from the first (1991ApJS...75..407M) and second (1991ApJS...76.1085M) papers, we now have accurate emission-line intensities for a total of 147 nebulae in the Magellanic Clouds. This sample contains a large selection of objects of low luminosity, with measurements of line intensities down to ~10% of H{beta}. Brighter objects have line intensities measured down to ~2% of H{beta}. Agreement with other authors is generally very good, especially for lines greater than approximately 10% of H{beta}. Reddening estimates from Balmer line ratios have been determined: unreddened and reddened line intensities are tabulated.
Uncorrected and corrected line intensity Lambda Wavelength 0.1nm ID Identification of wavelength --- PN Planetary nebula name --- Io(Lambda) Uncorrected line intensity (I(Hbeta)=100) --- n_Io(Lambda) s: saturated --- Ic(Lambda) Corrected line intensity (I(Hbeta)=100) --- n_Ic(Lambda) s: saturated --- Patricia Bauer CDS 1996 Oct 03 Pierre Leisy <leisy@iap.fr> J_ApJS_83_87.xml Surface Photometry of the Hydra I Cluster of Galaxies. I. Photometric Data. J/ApJS/85/249 J/ApJS/85/249 Surface Photometry of Hydra I Galaxies. I. Surface Photometry of the Hydra I Cluster of Galaxies. I. Photometric Data. M Hamabe Astrophys. J. Suppl. 85 249 1993 1993ApJS...85..249H Clusters, galaxy Galaxies, photometry Surface photometry was made for 137 galaxies on a UK Schmidt plate whose center is located at the center of the Hydra I (A1060) cluster of galaxies. For 133 of 137 galaxies the photometric parameters such as total magnitude, equivalent radius, concentration indices, and mean surface brightness were obtained. The total magnitudes were compared with those in the literature to check the accuracy of the present data. The estimated accuracy in the total magnitudes is about 0.1 mag at most for majority of the galaxies. This catalog is an updated version from the published paper.
Catalog of Bright Galaxies in Hydra I Seq Sequential number --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin A(EUSB) Major-axis diameter in EUSB The ESO/Uppsala Survey of the ESO(B) Atlas (Lauberts 1982) 0.1arcmin u_A(EUSB) Uncertainty flag for A(EUSB) --- B(EUSB) Minor-axis diameter in EUSB 0.1arcmin u_B(EUSB) Uncertainty flag for B(EUSB) --- Name Principal name of galaxy ESO designation is written FFFoo-NNN, where FFF = Field (plate) number, oo = Object class with G = galaxy IG = interacting galaxy NNN = number within field --- OtherID Alternative name(s) of galaxy --- ESO-LV Galaxy no. in ESO-LV cat. The Surface Photometry Catalogue of the ESO-Uppsala Galaxies (Lauberts & Valentijn 1989) --- Type Morphological type --- T Type index --- T(ESO) Type index taken from ESO-LV catalog --- V Helio-centric radial vel. from ESO-LV km/sec Member Membership B = background F = foreground --- u_Member Uncertainty flag for membership --- IRAS IRAS galaxy name --- B(VCC) Total B-mag.(Smyth & Stobie) Smyth and Stobie (1980: MNRAS, 190, 631) mag V(VCC) Total V-mag. from B(VCC) mag V25(Smy) Smyth's V_25 -Richter (1989) Richter (1989: A&AS, 68, 427) mag VT(RC3) Total V-mag. from RC3 mag BT(ESO) Total B-mag. from ESO-LV mag logRe Log of the effective equivalent radius arcsec u_logRe Uncertainty flag for logRe --- Mue Effective equiv. surf. bright. mag/arcsec2 u_Mue Uncertainty flag for Mue --- VT Total V-magnitude Total magnitude obtained by extrapolation of the V-band equivalent luminosity profile mag u_VT Uncertainty flag for VT --- D25 Major diameter at Mu = 25 arcsec u_D25 Uncertainty flag for D25 --- R25 Axial ratio, d25/D25 --- u_R25 Uncertainty flag for R25 --- SBe Mean surface brightness within Re calculated by the formula SBe = VT + 5 * logRe + 10.886 mag/arcsec2 u_SBe Uncertainty flag for SBe --- C21 Concentration index C21 = Re/R1 R1 is the equivalent radius corresponding to 1/4 total luminosity --- u_C21 Uncertainty flag for C21 --- C32 Concentration C32 = R3/Re R3 is the equivalent radius corresponding to 3/4 total luminosity --- u_C32 Uncertainty flag for C32 --- klim Lum. fraction above Mu_lim Mu_lim = 25.92 mag/arcsec**2 is the limit of the surface photometry --- k25 Lum. fraction above Mu = 25 --- V25 Isophotal magnitude V25 mag u_V25 Uncertainty flag for V25 --- VT2 Total V-mag. from integration mag u_VT2 Uncertainty flag for VT25 --- Masaru Hamabe IoA, U. Tokyo Nancy G. Roman, NSSDC/ADC 1994 Aug 04 J_ApJS_85_249.xml The structure of the core of 47 Tucanae from Hubble Space Telescope observations J/ApJS/85/293 J/ApJS/85/293 Structure of the core of 47 Tucanae from Hubble The structure of the core of 47 Tucanae from Hubble Space Telescope observations G De Marchi F Paresce F R Ferraro Astrophys. J. Suppl. Ser. 85 293 1993 1993ApJS...85..293D globular clusters: individual (47 Tuc) Hertzsprung-Russell (HR diagram) stars: luminosity function, mass function techniques: image processing *** No Description Available ***
HST
Stellar photometry: U band ID ID number --- X X position form the lower left corner of Fig.4 pix Y Y position form the lower left corner of Fig.4 pix m342 HST instrumental magnitude of all the 3567 stars detected and measured on the 44" x 44" U-band image named Fig.4 mag Stellar photometry: F220W and U bands ID ID number --- X X position as in table1 pix Y Y position as in table1 pix m220 HST instrumental magnitudes of all the 391 stars measured on the summed FOC F220W filter frame named Fig.3 mag m342 Corresponding m342 magnitude mag Stellar photometry: F140W, F220W and UBV bands ID ID number --- X X position pix Y Y position pix m140 magnitude at 140 nm mag m220 magnitude at 220 nm mag m342 m342 magnitude mag B B magnitude mag V V magnitude mag Patricia Bauer CDS 1994 Jun 24 Guido De Marchi <stscic::demarchi> J_ApJS_85_293.xml Rotation and Chromospheric emission among F, G and K dwarf stars of the Pleiades J/ApJS/85/315 J/ApJS/85/315 F, G and K dwarf stars of the Pleiades Rotation and Chromospheric emission among F, G and K dwarf stars of the Pleiades D R Soderblom J R Stauffer J D Hudon B F Jones Astrophys. J. Suppl. Ser. 85 315 1993 1993ApJS...85..315S Clusters, open Colors Effective temperatures Rotational Spectral types Stars, F-type Stars, G-type Stars, K-type *** No Description Available ***
A Census of F, G, and K Dwarf Members of the Pleiades fgk Running number number=1 Our running number, grouped in intervals of 0.1 in (B-V)0 [dereddened (B-V) color] and with a prefix roughly indicative of spectral class. These numbers are continued for the Pels stars i in Table 7b. --- Name Other names number=2 Star name: No prefix: H II number of Hertzsprung (1947). R, S: Trumpler (1922). Sometimes denoted as TR or TS. sk: Stauffer et al. 1991. Ton: Tonantzintla number from Haro et al. (1982). These are the numbers in column (1) of their Table I, and should not be confused with the `T' designations there. --- (B-V) Mean observed value number=3 Mean observed (B-V) value, taken from the compilation of Mermilliod (1986), except that any Johnson & Mitchell (1958) observation with (B-V) > 1.00 was rejected as being too inaccurate unless no other was available. Values with a colon indicate a poor-quality observation of Johnson & Mitchell (indicated by a `J' in column (4)) or that the (B-V) values for that star show greater than average variance. mag u_(B-V) Uncertainty flag (:) on (B-V) --- n Number of measurements or J number=4 Number of independent (B-V) values used to calculate col. (3). A `J' indicates that the only available datum was a photographic (B-V) from Johnson & Mitchell. --- (V-R)J Johnson color number=5 Johnson colors from Mendoza (1967) and Landolt (1979). mag (V-I)J Johnson color number=5 Johnson colors from Mendoza (1967) and Landolt (1979). mag (V-R)K Kron color number=7 Kron colors from Stauffer (1980, 1982, 1984). mag (V-I)K Kron color (7), or (b-y) if n_(V-I)K is ')' mag n_(V-I)K '(' indicates (V-I)K contains (b-y) number=8 for the hottest stars, Stroemgren index from Crawford and Perry (1976) --- (V-B)W Walraven from van Leeuwen et al. (1986). mag Sp Spectral type number=10 Spectral type, from Mermilliod (1986), Kraft & Greenstein (1969), Wilson (1963), Herbig (1962), Breger (1984), and Breger (1986). --- (B-V)0 Adopted unreddened color number=11 Adopted unreddened color, (B-V)0. Except for the few stars with unusual reddening (see Table 9), these were all calculated using E(B-V) = 0.04 magnitude, but all available colors were used as input, using mean relations. These colors are not, of course, precise to 0.001 magnitude but we have preserved an extra decimal place to reduce round-off error. mag u_(B-V)0 Uncertainty flag (:) on (B-V)0 --- Teff Adopted effective temperature number=12 Adopted value of the effective temperature, calculated from (B-V)0 as described in the text, and rounded to the nearest 20 K. K u_Teff Uncertainty flag (:) on Teff --- l_vsini Limit flag (<) on vsini, 'S' indicates a double-lined spectroscopic binary (SB2), --- vsini Rotational velocity number=13 Rotational velocity, from the present study, SH, Stauffer et al. 1984, Anderson et al. (1966), and Kraft (1967). A note of 'S' indicates a double-lined spectroscopic binary whose v sin i values are given in Table 2. A few other recent determinations of v sin i for some of these stars are mentioned in the text. km/s u_vsini Uncertainty flag (:) on vsini --- Pleiades members from Pels' list (A&A43, 423, 1975) fgk Running number, continued from table 7a. --- Pels number. --- (V-B)W Walraven color. mag (B-V)0 Estimated unreddened color. mag Francois Ochsenbein CDS 1994 Jan 15 David Soderblom <drs@stsci.edu> References: Anderson C., Stoeckly R., & Kraft R.P. 1966, ApJ, 143, 299 Breger M. 1984, A&AS, 57, 217 Breger M. 1986, ApJ, 309, 311 Crawford D.L. and Perry C.L. 1976, AJ, 81, 419 Haro G., Chavaria E., & Gonzalez G. 1982, Bol. Inst. Tonantzintla, 3, 1 Herbig G.H. 1962, ApJ, 135, 736 Hertzsprung E. 1947, Ann. Leiden Obs., 19, Part 1A Johnson H.L. & Mitchell R.I. 1958, ApJ, 128, 31 Kraft R.P. 1967, ApJ, 150, 551 Kraft R.P. & Greenstein J.L. 1969, in Low-Luminosity Stars, ed. S.S. Kumar (New York: Gordon & Breach), 65 Landolt A.U. 1979, ApJ, 231, 468 Mendoza E.E. 1967, Bol. Obs. Tonantzintla y Tacubaya, 4, 149 Mermilliod J.-C. 1986, Bull. D'Inf. du CDS, No. 31, 175 Stauffer J.R. 1980, AJ, 85, 1341 Stauffer J.R. 1982, AJ, 87, 1507 Stauffer J.R. 1984, ApJ, 280, 189 Stauffer J.R., Hartmann L.W., Soderblom D.R., & Burnham J.N. 1984, ApJ, 280, 202 Stauffer J.R., Klemola A., Prosser C., & Probst R. 1991, AJ, 101, 980 Trumpler R.J. 1922, Lick Obs. Bull. 10, 110 van Leeuwen F., Alphenaar P., & Brand J. 1986, A&AS, 65, 309 Wilson O.C. 1963, ApJ, 138, 832 J_ApJS_85_315.xml The Case Low-Dispersion Northern Sky Survey. XIV. A-F Stars in a Region in Southern Canes Venatici J/ApJS/86/453 J/ApJS/86/453 Case Low-Dispersion Survey. XIV. The Case Low-Dispersion Northern Sky Survey. XIV. A-F Stars in a Region in Southern Canes Venatici D J MacConnell C B Stephenson P Pesch Astrophys. J. Suppl. Ser. 86 453 1993 1993ApJS...86..453M Stars, halo Stars, horizontal branch Surveys Positions and estimated magnitudes are provided for 387 A-F stars in an 190 square degree region in southern Canes Venatici. The area encompassed is between R.A. 12h00m and 14h10m and Decl. +29deg00' and +38deg30'(1950), excluding the region R.A. 12h00m to 13h00m and Decl. +29deg to +34deG, which was covered in a previous paper. The A-F stars, whose blue magnitudes are within the range 8 through 18 (median 14), were identified on low-dispersion objective-prism plates taken with Case Western Reserve University's Burrell Schmidt telescope at Kitt Peak.
List of A-F stars in Southern CVn A-F + Number --- n_A-F Additional remark --- RAh Right Ascension(1950) h RAm Right ascension(1950) min RAs Right Ascension(1950) s uRAs Uncertainty flag on RA --- DEd Declination(1950) deg DEm Declination(1950) arcmin u_DEm Uncertainty flag on DE --- mB Blue magnitude mag Sp Spectral Classification --- Quality Quality of spectral type --- Remarks Remarks and Cross Identifications --- P. Pesch Case Western Reserve University 1994 Jul 18 J_ApJS_86_453.xml Mid- and far-infrared spectroscopy of ices: optical constants and integrated absorbances J/ApJS/86/713 J/ApJS/86/713 IR spectroscopy of ices Mid- and far-infrared spectroscopy of ices: optical constants and integrated absorbances D M Hudgins S A Sandford L J Allamandola A G G M Tielens Astrophys. J. Suppl. Ser. 86 713 1993 1993ApJS...86..713H line: identification molecular data Laboratory spectra through the mid-infrared (4000 to 500cm^-1 [2.5-20 micron]) have been used to calculate the optical constants (n and k) and integrated absorption coefficients (A) for a variety of pure and mixed molecular ices of relevance to astrophysics. The ices studied were H2O, CH3OH, CO2, OCS, CH4, CO2+CH4, CO2+OCS, CO+CH4, CO+OCS, O2+CH4, O2+OCS, N2+CH4, N2+OCS, H2O+CH4, H2O+OCS, and H2O+CH3OH+CO+NH3. In addition, the measurements have been extended through the far-infrared (500 to 50cm^1 [20-200 micron]) for the H2O, CH3OH, and H2O+CH3OH+NH3 ices.
H2O:CH3OH:CO:NH3 = 100:10:1:1 Ice Mixture (Weak Interstellar Mix) percentage transmission H2O:CH3OH:CO:NH3 = 100:50:1:1 Ice Mixture (Strong Interstellar Mix) percentage transmission Pure CH3OH Ice percentage transmission Pure H2O Ice percentage transmission Pure CH4 Ice percentage transmission Pure CO2 Ice percentage transmission Pure OCS Ice percentage transmission CO:CH4 = 20:1 Ice Mixture percentage transmission CO:OCS = 20:1 Ice Mixture percentage transmission CO2:CH4= 20:1 Ice Mixture percentage transmission CO2:OCS= 20:1 Ice Mixture percentage transmission H2O:CH4= 20:1 Ice Mixture percentage transmission H2O:OCS= 20:1 Ice Mixture percentage transmission H2O:OCS= 2:1 Ice Mixture percentage transmission N2:CH4 = 20:1 Ice Mixture percentage transmission N2:OCS = 20:1 Ice Mixture percentage transmission O2:CH4 = 20:1 Ice Mixture percentage transmission O2:OCS = 20:1 Ice Mixture percentage transmission Temp Temperature K nu Frequency cm-1 %T Percentage of transmission % H2O:CH3OH:CO:NH3 = 100:10:1:1 Ice Mixture (Weak Interstellar Mix) optical constants H2O:CH3OH:CO:NH3 = 100:50:1:1 Ice Mixture (Strong Interstellar Mix) optical constants Pure CH3OH Ice optical constants Pure H2O Ice optical constants Pure CH4 Ice optical constants Pure CO2 Ice optical constants Pure OCS Ice optical constants CO:CH4 = 20:1 Ice Mixture optical constants CO:OCS = 20:1 Ice Mixture optical constants CO2:OCS = 20:1 Ice Mixture optical constants H2O:CH4 = 20:1 Ice Mixture optical constants H2O:OCS = 20:1 Ice Mixture optical constants H2O:OCS = 2:1 Ice Mixture optical constants N2:CH4 = 20:1 Ice Mixture optical constants N2:OCS = 20:1 Ice Mixture optical constants O2:CH4 = 20:1 Ice Mixture optical constants O2:OCS = 20:1 Ice Mixture optical constants Temp Temperature K nu Frequency cm-1 n Real part of the index of refraction number=1 The index of refraction is the complex number n + ik --- k Imaginary part of the index of refraction --- CO2:CH4 = 20:1 Ice Mixture optical constants Temp Temperature K nu1 Frequency nu1 cm-1 n(nu1) Real part of the index of refraction for frequency nu1 number=1 The index of refraction is the complex number n + ik --- nu2 Frequency nu2 cm-1 k(nu2) Imaginary part of the index of refraction for frequency nu2 --- Patricia Bauer CDS 1994 Sep 16 J_ApJS_86_713.xml New OH/IR stars from color-selected IRAS sources. III. A complete survey J/ApJS/89/189 J/ApJS/89/189 IRAS PSC new OH/IR stars. III. New OH/IR stars from color-selected IRAS sources. III. A complete survey J N Chengalur B M Lewis J Eder Y Terzian Astrophys. J. Suppl. Ser. 89 189 1993 1993ApJS...89..189C II/125 : IRAS Point Source Catalogue, Version 2.0 (IPAC 1986) J/A+AS/90/327 : IRAS Point Source 1612MHz OH survey (te Lintel Hekkert+ 1991) Eder J. et al., Paper I, =1988ApJS...66..183E Lewis et al., Paper II, =1990ApJ...362..634 Infrared sources Radio lines infrared: stars radio lines: stars stars: AGB and post-AGB surveys We present the results of 1612MHz observations conducted at the Arecibo Observatory of 571 color-selected sources from the IRAS Point Source Catalog. Of these sources we detect 132, 113 for the first time. This is the third part of an Arecibo survey of color-selected IRAS sources. The earlier two parts together detected a total of 268 sources of 1612MHz emission. An analysis of the properties of the OH/IR stars detected in all three parts of the survey is included. In particular we compute the limiting 1612MHz peak flux of the entire survey to be ~40mJy. The correlation between the IRAS infrared fluxes and the 1612MHz flux of the 132 sources detected in part III of the survey is smaller than that found in the earlier parts of the survey. This is to be expected from the intrinsic variability of OH/IR stars and the longer time gap between the 1612MHz observations and the IRAS measurements. We identify a subset of 54 stars as being near the tangent point of the galactic rotation curve. Using the kinematical distances to these stars we find that the efficiency of momentum transfer varies exponentially with the (25-12){mu}m color, consistent with the stellar outflow being driven by radiation pressure. Further the IR pump efficiency increases with increasing optical depth of the circumstellar shell, as expected for radiative pumping. The bolometric luminosity function is found to decrease sharply above L_Bol_=5600L_{sun}_, and the 1612MHz luminosity function shows a corresponding falloff above L_1612_=1.8x10^-8^L_{sun}_. We also find direct confirmation of the expectation that sources with large expansion velocity are more luminous than sources with small expansion velocity.
Detections IRAS IRAS name --- m_IRAS Multiplicity index on IRAS name --- n_IRAS Note on IRAS name number=1 *: OH source not listed in the compilation by te Lintel Hekkert et al., 1989A&AS...78..399T --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec S1612MHz Total integrated 1612MHz flux mJy.km/s S1612-l Integrated 1612MHz flux in the low-velocity half of the spectrum mJy.km/s S1612-h Integrated 1612MHz flux in the high-velocity half of the spectrum mJy.km/s DV(100) Velocity separation between the half-power points of the two peaks in the line profile {DELTA}V_100_ km/s DV(50) Velocity separation between the half-power points of the two peaks in the line profile {DELTA}V_50_ km/s u_DV(50) Uncertainty flag on DV(50). --- Vl LSR velocity of the low-velocity peak km/s Vh LSR velocity of the high-velocity peak km/s <V> Systemic LSR velocity km/s (25-12) (25-12){mu}m infrared color mag (60-25) (60-25){mu}m infrared color mag Name Other name, if the source corresponds to one known before the IRAS survey --- Non-detections IRAS IRAS name --- GLON Galactic longitude deg GLAT Galactic latitude deg (12-25) (12-25){mu}m infrared color mag (60-25) (60-25){mu}m infrared color mag James Marcout, Patricia Bauer CDS 1996 Nov 28 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_89_189.xml Far-ultraviolet stellar photometry: a field in Orion J/ApJS/89/259 J/ApJS/89/259 Far-UV photometry in Orion Far-ultraviolet stellar photometry: a field in Orion E G Schmidt G R Carruthers Astrophys. J. Suppl. Ser. 89 259 1993 1993ApJS...89..259S J/ApJ/408/484 : (Another observation in a field in Monoceros) Photometry, ultraviolet Far-ultraviolet photometry for 625 objects in Orion is presented. These data were extracted from electrographic camera images obtained during sounding rocket flights in 1975 and 1982. The 1975 images were centered close to the belt of Orion while the 1982 images were centered approximately 9 deg further north. One hundred and fifty stars fell in the overlapping region and were observed with both cameras. Sixty-eight percent of the objects were tentatively identified with known stars using the SIMBAD database while another 24% are blends of objects too close together to separate with the resolution used.
Objects detected in the UV No Number of the star --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin m1367 Far UV magnitude mag m1519 Far UV magnitude mag Name Identification (from SIMBAD) of the star --- mag V or P magnitude mag n_mag P if mag is photographic --- Sp Spectral type --- Francois Ochsenbein CDS 1993 Dec 23 Edward Schmidt (eschmidt@unlinfo.unl.edu) J_ApJS_89_259.xml A catalog of blue and red supergiants in M33. J/ApJS/89/85 J/ApJS/89/85 Blue and red supergiants in M33 A catalog of blue and red supergiants in M33. G R Ivanov W L Freedman B F Madore Astrophys. J. Suppl. Ser. 89 85 1993 1993ApJS...89...85I Photometry, UBV Stars, blue Stars, supergiant catalogs galaxies: individual (M 33) galaxies: stellar content supergiants techniques: photometric We present a catalog of blue and red stars in M33 based on photographic photometry of over 65,000 objects extracted from plates taken with the 3.6m Canada-France-Hawaii Telescope (CFHT) and the 2.0m Rozhen (Bulgarian) Telescope. The completeness limit of the various surveys are estimated here to be V=19.5mag for those stars situated in crowed associations, and V=20.0mag for stars in the interarm fields. We list magnitudes and positions for 2112 blue stars, defined by (U-V)<0.0mag, and V<19.5mag, and 389 red stars defined by (B-V)>1.8mag and V<19.5mag. Of these, 1156 are candidate O stars on the basis of (U-V)<-0.9mag.
Catalog of blue stars in M 33 The bright blue stars in M33 with V < 17.0 A subset of multiple objects from Table 2 A subset of nonstellar objects from Table 2 A subset of candidate WR stars from Table 2 IFM-B += Running number assigned according to increasing right ascension --- m_IFM-B Multiplicity index on IFM-B --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Vmag Photographic V magnitude mag B-V B-V colour index mag U-B U-B colour index mag Rem Remarks number=1 B: a blue star as catalogued and numbered in Humphreys & Sandage (1980ApJS...44..319H n: nonstellar (probably a cluster or H II region in M 33 M: multiple object WR: candidate Wolf-Rayet star --- Assoc. Number of the OB association in which the object can be found --- Assoc.2 Second association number when the object is in two ones --- Fig Number of figures (Figs 5-11; Figs12-22) on which the object can be identified --- A catalog of red stars in M33 IFM-R Sequential number --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Vmag Photographic V magnitude mag B-V B-V colour index mag Rem Remarks number=1 R: a red star as catalogued and numbered in Humphreys & Sandage (1980ApJS...44..319H) Q: Object of unknown nature Humphreys & Sandage (1980ApJS...44..319H) B: a blue star as catalogued and numbered in Humphreys & Sandage (1980ApJS...44..319H) --- Fig Number of figures on which the object can be identified --- Patricia Bauer CDS 1996 Nov 12 Barry Madore <barry@ipac.caltech.edu> J_ApJS_89_85.xml The Parkes-MIT-NRAO (PMN) map catalog of radio sources covering -88 deg < dec. < -37 deg at 4.85 GHz J/ApJS/90/173 J/ApJS/90/173 PMN map catalog of radiosources The Parkes-MIT-NRAO (PMN) map catalog of radio sources covering -88 deg < dec. < -37 deg at 4.85 GHz P C Gregory J D Vavasour W K Scott J J Condon Astrophys. J. Suppl. Ser. 90 173 1994 1994ApJS...90..173G catalogs radio continuum: general surveys The Parkes-MIT-NRAO (PMN) Southern Survey was made with the NRAO 4.85 GHz seven-beam receiver on the Parkes 64 m telescope during 1990 June (Griffith, M., & Wright, A. E. 1993, AJ, 105, 1666), and maps covering the 2.5 sr declination band -88 deg to -37 deg were constructed from the survey scans (Condon, J. J., Griffith, M., & Wright, A. E. 1993, AJ, 106, 1095). The PMN map catalog of 15,045 discrete sources with angular sizes <15arcmin and stronger than S~25mJy was derived from these maps (Gregory, P. C., Vavasour, J. D., Scott, W. K., & Condon, J. J. 1994, ApJS, 90, 173). A printed version of this catalog with B1950 coordinates is available from the NRAO. There are two machine-readable versions of the PMN map catalog, with coordinates precessed to B1950 (file B1950) and J2000 (file J2000). Each catalog file contains one line per source (15,045 lines each), and the sources are sorted by increasing B1950 or J2000 right ascension. The Parkes-MIT-NRAO (PMN) southern survey was made with the NRAO 4.85GHz seven-beam receiver on the Parkes 64 m telescope during 1990 June, and maps covering the Omega = 2.5 sr declination band -88deg<Dec.<-37deg were constructed from the survey scans. We present a catalog of 15,045 discrete sources with angular sizes phi<~15arcmin and stronger than S~25mJy derived from these maps. Machine-readable versions of the catalog with either B1950 or J2000 positions, and a printed catalog with B1950 positions only, are available. The 4.85GHz weighted source counts S^(5/2)^n(S) between 30mJy and 10Jy were obtained and agree well with previous results.
PMN catalog, B1950 coordinates RAh Right ascension B1950 h RAm Right ascension B1950 min RAs Right ascension B1950 s e_RAs rms uncertainty in RA s DE- Declination sign --- DEd Declination B1950 deg DEm Declination B1950 arcmin DEs Declination B1950 arcsec e_DEs rms uncertainty in DE arcsec GLAT Galactic latitude deg GLON Galactic longitude deg Flux 4.85 GHz peak flux density mJy e_Flux rms uncertainty in peak flux density mJy n1_Flux 'E' for significant extension --- n2_Flux 'W' for warning --- n3_Flux 'C' for confusion --- MajAxis Fitted major axis / beam size --- MinAxis Fitted minor axis / beam size --- PosAng Fitted major axis position angle (degrees east of north) deg Z Local sky level (per beam) mJy Map_X Map pixel column number (from left) --- Map_Y Map pixel row number (from bottom) --- PMN catalog, J2000 coordinates RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s e_RAs rms uncertainty in RA s DE- Declination sign J2000 --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec e_DEs rms uncertainty in DE arcsec GLAT Galactic latitude deg GLON Galactic longitude deg Flux 4.85 GHz peak flux density mJy e_Flux rms uncertainty in peak flux density mJy n1_Flux 'E' for significant extension --- n2_Flux 'W' for warning --- n3_Flux 'C' for confusion --- MajAxis Fitted major axis / beam size --- MinAxis Fitted minor axis / beam size --- PosAng Fitted major axis position angle (degrees east of north) deg Z Local sky level (per beam) mJy Map_X Map pixel column number (from left) --- Map_Y Map pixel row number (from bottom) --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 27-Oct-1994 Apr 15 AAS CD-ROM series, Volume 2, 1994 Addresses: Gregory P.C., Vavasour J.D. and Scott W.K. Physics Department, University of British Columbia, Vancouver, BC, V6T 2A6, Canada Condon J.J. National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 J_ApJS_90_173.xml A search for binaries in the globular cluster NGC 3201 J/ApJS/90/83 J/ApJS/90/83 Binaries in NGC 3201 A search for binaries in the globular cluster NGC 3201 P Cote D L Welch P Fischer G S Da Costa P Tamblyn P Seitzer M J Irwin Astrophys. J. Suppl. Ser. 90 83 1994 1994ApJS...90...83C Clusters, globular Photometry, CCD Radial velocities We present BV CCD and APM photometry, accurate astrometry and 1859 radial velocities for 1318 stars within ~36deg of the Galactic globular cluster NGC 3201. The field and cluster populations separate unambiguously in two distinct samples since the systemic radial velocity of NGC 3201 is 494.2km/s. After removal of the 19 known NGC 3201 photometric variables in our sample, we have a database of 930 radial velocities for 420 member giants (276 of which have multiple velocity measurements) with which to identify spectroscopic binaries on the basis of radial velocity variations. The mean time span of the observations is 1.7yr, with coverage up to ~6yr for our best-studied stars. Monte Carlo simulations of the observed velocity variations have provided _upper_limits_ to the cluster binary fraction (for binaries with 0.1<=P<=5-10yr and mass ratios in the range 0.1-1) of 0.06-0.10 (circular orbits) and 0.15-0.18 (eccentric orbits). These results suggest an incidence of binarism for NGC 3201 consistent with the corresponding incidence among nearby solar-type stars having similar periods and mass ratios (0.04-0.08) and that for a small sample of other globular clusters (0.05-0.12) studied by Hut et al. (1992PASP..104..981H). The detailed analysis of the cluster dynamics, based on the data given here, are presented by Cote et al. (1995ApJ...454..788C).
Radial velocities for photometric variables VarID Star number in this table number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) --- RAh Right Ascension J2000 (hours) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) h RAm Right Ascension J2000 (minutes) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) min RAs Right Ascension J2000 (seconds) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) s DE- Declination J2000 (sign) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) --- DEd Declination J2000 (degrees) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) deg DEm Declination J2000 (minutes) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) arcmin DEs Declination J2000 (seconds) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) arcsec HJD Heliocentric Julian Date of observation number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) d RVel Radial velocity number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) km/s e_RVel Mean error on RVel number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) km/s Period Period of variability it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) d r_RVel Source of velocity the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) --- ID(Saw) Designation in Sawyer-Hog (1973) Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) number= it is taken from Fourcade & Laborde (1966, Atlas y Catalogo de Estrellas Variables en Cumulos Globulares al sur de 29deg, La Plata, Asociacion Argentina de Astronomia, or Sawyer-Hogg (1973, Publ. Dominion Astrophys. Obs. Victoria, =1973PDDO....3....6S) number= the code refers to telescope and instrument, see column 4 of table 1 in the printed paper number= Variable designation in Sawyer-Hogg's 1973 paper (1973PDDO....3....6S) --- Radial velocities and photometry Star Star identification number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Dist Distance from cluster center arcmin HJD HJD of radial velocity observation d RV Heliocentric radial velocity km/s e_RV RV uncertainty km/s RVmean Weighted mean heliocentric radial velocity km/s e_RVmean RVmean uncertainty km/s Vmag Apparent V magnitude mag B-V Apparent B-V color mag o_RV Number of radial velocity measurements --- 2_RV Chi-square for radial velocities --- Chi2RV Reduced chi-square for radial velocities --- Prob Probability of obtaining a chi-square at least this large purely as a consequence of measurement error --- Src Source of photometry, 'APM' or 'CCD' --- Radial velocities for NGC 3201 field stars ID Identification number --- n_ID '*' if identified as member in another run --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s DE- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec Dist Distance from cluster center arcmin HJD Heliocentric Julian date of observation d RV Heliocentric Radial Velocity km/s e_RV rms uncertainty on RV km/s Vmag V Magnitude mag B-V B-V Colour mag Phot Source of Photometry (APM or CCD) --- ObsRun Observing Run number=1 LC = Las Campanas; A1/A2 = CTIO + ARGUS --- Lee Brotzman ADS 1994, rev. CDS Staff [CDS] 15-Oct-1996 Apr 09 AAS CD-ROM series, Volume 2, 1994; table2 added at CDS (15-Oct-1996) Addresses: Cote P., Welch D.L. and Fischer P. Department of Physics and Astronomy, McMaster University, Hamilton, ON, Canada L8S 4M1 Da Costa G.S. Anglo-Australian Observatory, P.O. Box 296, Epping, NSW 2121, Australia Tamblyn P. Steward Observatory, University of Arizona, Tucson, AZ, 85721 Seitzer P. Department of Astronomy, University of Michigan, Ann Arbor, MI, 48109 Irwin M.J. Royal Greenwich Observatory, Madingley Road, Cambridge, CB3 0HA, UK J_ApJS_90_83.xml A 5GHz VLA survey of the galactic plane. J/ApJS/91/347 J/ApJS/91/347 A 5-GHz VLA Survey of the Galactic Plane A 5GHz VLA survey of the galactic plane. R H Becker R L White D J Helfand S Zoonematkermani Astrophys. J. Suppl. Ser. 91 347 1994 1994ApJS...91..347B II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) H II regions Infrared sources Planetary nebulae Radio sources HII regions planetary nebulae: general radio continuum: galaxies surveys We have used the VLA to survey the inner Galaxy (|b|<0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.
5 GHz and 1.4GHz sources in the inner Galaxy Name5GHz 5 GHz name (LLL.lll+B.bbb) --- RAh Right ascension (1950) at 5GHz h RAm Right ascension (1950) at 5GHz min RAs Right ascension (1950 at 5GHz s DE- Declination sign --- DEd Declination (1950) at 5GHz deg DEm Declination (1950) at 5GHz arcmin DEs Declination (1950) at 5GHz arcsec l_Sp5GHz Limit flag on Sp5GHz --- Sp5GHz Peak flux density at 5GHz number=1 The values of Speak and Sint have been corrected for the loss of sensitivity of the primary beam of the antennas away from the field centre. mJy l_Si5GHz Limit flag on Si5GHz --- Si5GHz Integrated flux density at 5GHz number=1 The values of Speak and Sint have been corrected for the loss of sensitivity of the primary beam of the antennas away from the field centre. mJy Diam5GHz Source diameter at 5GHz number=2 The quoted diameters are the mean of the best-fit FWHM of the major and minor axes of the sources as determined by the Gaussian fits. arcsec n_Diam5GHz CD: the 5GHz source was observed in the CnD configuration --- Name1.4GHz 1.4 GHz name (LLL.lll+B.bbb) --- n_Name1.4GHz N: new source (Not in 1.4GHz catalog) --- Sp1.4GHz Peak flux density at 1.4GHz number=1 The values of Speak and Sint have been corrected for the loss of sensitivity of the primary beam of the antennas away from the field centre. mJy Si1.4GHz Integrated flux density at 1.4GHz number=1 The values of Speak and Sint have been corrected for the loss of sensitivity of the primary beam of the antennas away from the field centre. mJy n_Si1.4GHz +: the flux was measured using IMEAN --- Diam1.4GHz Source diameter at 1.4GHz number=2 The quoted diameters are the mean of the best-fit FWHM of the major and minor axes of the sources as determined by the Gaussian fits. arcsec Mult ": Multiple 1.4GHz sources associated with the 5GHz source --- Com Comments number=3 I: Has a likely counterpart in the IRAS PSC i: Has a low probability IRAS PSC match *: Source is part of a group, integrated flux includes another nearby source (also marked with *) MLNSO(name): Master List of Non-Stellar Objects PN l+b: Strasbourg Catalog of Planetary Nebulae (Cat. <V/84>) SNR: Associated with a supernova remnant SNR?, PN?: May be either PN or a SNR TX=fff: Texas 0.365 GHz (Cat. <VIII/42>) source, fff = flux in mJy XR: X-ray source in Einstein IPC catalog int=xxx: Large extended source, xxx = integrated flux in mJy --- IRAS-selected ultracompact H II regions IRAS-selected planetary nebulae Other High-probability 6cm/IRAS sources Low-probability 6cm/IRAS matches GPS GPS name --- S6cm Flux density at 6 cm (5GHz) mJy Diam Source diameter arcmin IRAS IRAS name --- m_IRAS Multiplicity index on IRAS --- l_S12um Limit flag on S12um --- S12um Flux density at 12{mu}m mJy l_S25um Limit flag on S25um --- S25um Flux density at 25{mu}m mJy l_S60um Limit flag on S60um --- S60um Flux density at 60{mu}m mJy l_S100um Limit flag on S100um --- S100um Flux density at 100{mu}m mJy Prob Probability % Type C: Candidate, A: Ambiguous --- Heinz Andernach, Francois Ochsenbein CDS 1997 Apr 25 UNKNOWN UNKNOWN Tables 4a and 4b were provided by R.L. White to H. Andernach (heinz@cuevano.ugto.mx) and archived as R106 in his catalogue collection. Tables 4c and 4d were prepared via OCR and proof-read by H. Andernach. J_ApJS_91_347.xml Extreme ultraviolet spectrum of a solar active region from SERTS J/ApJS/91/461 J/ApJS/91/461 EUV spectrum of solar active region Extreme ultraviolet spectrum of a solar active region from SERTS R J Thomas W M Neupert Astrophys. J. Suppl. Ser. 91 461 1994 1994ApJS...91..461T Spectra, ultraviolet Sun Sun: activity Sun: UV radiation We present wavelengths and absolute intensities for 269 emission lines from a single active region observed by the Solar EUV Rocket Telescope and Spectrograph (SERTS) on 1989 May 5. For this catalog, the imaged spectra have been spatially averaged over a field of view 7"x276" cutting through the center of AR5464 at S18 W45. Wavelength coverage is 170-450A with a spectral resolution approaching 10,000. Most of the line positions are determined to 5mA or better, representing the highest accuracy yet obtained for solar wavelengths throughout this spectral interval. The relative photometric calibration of the instrument is good to +/-20% over its first-order range, and has been placed onto an absolute scale that should be correct to within a factor less than 2. Where known, identifications, atomic transitions and formation temperatures are also given. The identified lines arise from temperatures that cover the range 4.7<=logT<=6.8, providing information about the Sun's corona and upper transition region. Upper limits to the intensity of any emission line not included here can be estimated from the measured instrumental sensitivity. This averaged EUV spectrum should prove useful as a source of accurate wavelengths and intensities for emission characteristic of the high-temperature plasma associated with a solar active region and small subflare.
Wavelength calibration results Cen Fitted line centroid 5upix SERTS Measured SERTS wavelength using calibration relationship 0.1nm Std Known wavelength of line standard 0.1nm Ion Ion of measured line standard --- Res Residual (SERTS - Std) 0.1pm Instrumental 3 sigma sensitivity levels versus wavelength (first and second order) Lam1 1st-order wavelength 0.1nm 3sig(1) 1st-order spectral intensity sensitivity (3-sigma) 10mW/m2/sr/nm 3L(1) 1st-order integrated intensity sensitivity (3-sigma) number=1 Values of 3L(1) and 3L(2) can be used as intensity upper limits for lines not listed in table3. mW/m2/sr Lam2 2nd-order wavelength 0.1nm 3sig(2) 2nd-order spectral intensity sensitivity (3-sigma) 10mW/m2/sr/nm 3L(2) 2nd-order integrated intensity sensitivity (3-sigma) number=1 Values of 3L(1) and 3L(2) can be used as intensity upper limits for lines not listed in table3. mW/m2/sr Solar active region EUV spectrum Lam Measured line wavelength 0.1nm n_Lam s = second-order line --- e_Lam 1-sigma uncertainty in Lambda 0.1pm I Measured integrated line intensity mW/m2/sr e_I 1-sigma uncertainty in I mW/m2/sr W Measured line full-width-half-maximum 0.1pm e_W 1-sigma uncertainty in W 0.1pm Ion Emitting ion (if known) --- n_Ion b = blend --- Behr Fractional part of wavelength reported by Behring et al. 1976 0.1nm Dere Fractional part of wavelength reported by Dere 1978 plus Feldman et al. 1987 0.1nm Kelly Fractional part of wavelength reported by Kelly 1987 0.1nm ID Identification code number=1 0 = Unidentified; 1 = Behring et al. 1976, ApJ, 203, 521 2 = Dere 1978, ApJ, 221, 1062 3 = Feldman et al. 1987, Atlas of Skylab EUV Spectroheliograms, Washington, DC: Naval Research Laboratory 4 = This work using Kelly 1987, J. Phys. Chem. Ref. Data, 16, Suppl., 1, 1371 5 = Keenan et al. 1991, ApJ, 379, 406 6 = Mason & Bhatia 1978, MNRAS, 184, 423 7 = Kastner 1991, Sol. Phys., 135, 343 8 = Behring 1992, private communication 9 = Monsignori-Fossi 1992, private communication --- Note Special note, see file notes3 --- Solar active region lines by ion Ion Emitting ion --- logT Temperature of maximum ionization abundance --- Lam Measured line wavelength 0.1nm n1_Lam s = second order line --- n2_Lam b = blend --- e_Lam 1-sigma uncertainty in Lambda 0.1pm I Measured integrated line intensity mW/m2/sr e_I 1-sigma uncertainty in I mW/m2/sr Config Electronic configurations involved in the emission transition --- Terms Electronic level terms involved in the emission transition --- IES Iso-electronic sequence of emitting ion --- TN Transition number for the emission line --- Number of lines by ion in solar active region EUV spectrum Z Atomic Z-number of emitting element --- Ion Chemical symbol of emitting element --- N(II) Number of lines observed from ionization stage II of element --- N(III) Lines from ionization stage III --- N(IV) Lines from ionization stage IV --- N(V) Lines from ionization stage V --- N(VI) Lines from ionization stage VI --- N(VII) Lines from ionization stage VII --- N(VIII) Lines from ionization stage VIII --- N(IX) Lines from ionization stage IX --- N(X) Lines from ionization stage X --- N(XI) Lines from ionization stage XI --- N(XII) Lines from ionization stage XII --- N(XIII) Lines from ionization stage XIII --- N(XIV) Lines from ionization stage XIV --- N(XV) Lines from ionization stage XV --- N(XVI) Lines from ionization stage XVI --- N(XVII) Lines from ionization stage XVII --- N(XVIII) Lines from ionization stage XVIII --- N(XIX) Lines from ionization stage XIX --- N(XX) Lines from ionization stage XX --- N(Total) Total number of lines observed from all ions of given element --- Unidentified lines in solar active region EUV spectrum Lam Measured line wavelength 0.1nm n_Lam s = all fields are interpreted as appearing in 2nd-order, otherwise they are in 1st-order --- e_Lam 1-sigma uncertainty in Lambda 0.1pm I Measured integrated line intensity mW/m2/sr e_I 1-sigma uncertainty in I mW/m2/sr W Measured line full-width-half-maximum 0.1pm e_W 1-sigma uncertainty in W 0.1pm Spectrum N*Wave Spectral order times Wavelength 0.1nm S Measured solar spectrum in Relative Exposure Units (REU) --- Ef Absolute Conversion Factor of REU, 1st-order 10mW/m2/sr/nm Es Absolute Conversion Factor, of REU 2nd-order 10mW/m2/sr/nm Pf Absolute Conversion Factor, of REU 1st-order 10ph/cm2/s/arcsec2/nm Ps Absolute Conversion Factor, of REU 2nd-order 10ph/cm2/s/arcsec2/nm So Raw spectral data, in REU --- Back Background, in REU --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 28-Oct-1994 May 11 AAS CD-ROM series, Volume 2, 1994 Addresses: Thomas R.J. and Neupert W.M. Laboratory for Astronomy and Solar Physics, Code 680, NASA-Goddard Space Flight Center, Greenbelt, MD 20771 J_ApJS_91_461.xml Surface photometry of low-luminosity radio galaxies J/ApJS/91/507 J/ApJS/91/507 Radio-galaxies surface photometry Surface photometry of low-luminosity radio galaxies L De Juan L Colina I Perez-Fournon Astrophys. J. Suppl. Ser. 91 507 1994 1994ApJS...91..507D galaxies: photometry galaxies: structure radio continuum: galaxies We present the results on the optical morphology and structure of 25 low-luminosity radio galaxies. The radial dependence of parameters like the surface brightness, ellipticity, center, and position angle of the isophotes is presented to study the properties of the galaxies. Results for individual objects are discussed.
Isophote fitting parameters Name Name number=1 When the name is followed by com, it is the companion galaxy --- Rad Radius arcsec SuBr Surface brightness mag/arcsec e_SuBr rms uncertainty on SuBr mag/arcsec Eps Ellipticity --- PAa Position angle of the major axis deg X0 Isophote center X coordinate pix Y0 Isophote center Y coordinate pix B4 Fourier coefficient of the term cos(4theta) 10-3 table2.tex LaTeX version of table2 Lee Brotzman ADS 1994, Patricia Bauer [CDS] 03-Nov-1994 Apr 25 AAS CD-ROM series, Volume 2, 1994 J_ApJS_91_507.xml The initial mass function for massive stars in the Magellanic Clouds. I. UBV photometry and color-magnitude diagrams for 14 OB associations J/ApJS/91/583 J/ApJS/91/583 MC massive stars IMF. I. The initial mass function for massive stars in the Magellanic Clouds. I. UBV photometry and color-magnitude diagrams for 14 OB associations R J Hill B F Madore W L Freedman Astrophys. J. Suppl. Ser. 91 583 1994 1994ApJS...91..583H Hertzsprung-Russell (HR diagram) Magellanic Clouds open clusters and associations: general stars: early-type stars: luminosity function, mass function UBV CCD photometry has been obtained for 14 OB associations in the Magellanic Clouds using the University of Toronto's 0.6m telescope and the Carnegie Institution of Washington's 1.0m reflector, both on Las Campanas, Chile. The data are presented and used to construct color-magnitude diagrams for the purposes of investigating the massive-star content of the associations.
UBV photometry Name OB association name (bytes 1-7) and star identification number (bytes 10-13) --- X X coordinate of star on CCD image in fig. 1 --- Y Y coordinate --- V V magnitude mag e_V rms uncertainty on V mag B-V B-V color mag e_B-V rms uncertainty on B-V mag U-B U-B color mag e_U-B rms uncertainty on U-B mag Lee Brotzman ADS 1994, Patricia Bauer [CDS] 03-Nov-1994 Apr 25 AAS CD-ROM series, Volume 2, 1994 Addresses: Hill R.J. hill@ociw.edu Department of Astronomy, University of Toronto, 60 St. George Street, Toronto, Ontario, Canada M5S 1A1 Madore B.F. barry@ipac.caltech.edu NASA/IPAC Extragalactic Database, Infrared Processing and Analysis Center, California Institute of Technology, Jet Propulsion Laboratory, MS 100-22, Pasadena, CA 91125 Freedman W.L. wendy@ociw.edu The Observatories, Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101 J_ApJS_91_583.xml A deep imaging survey of the Pleiades with ROSAT. J/ApJS/91/625 J/ApJS/91/625 ROSAT survey of the Pleaides A deep imaging survey of the Pleiades with ROSAT. J R Stauffer J -P Caillault M Gagne C F Prosser L W Hartmann Astrophys. J. Suppl. 91 625 1994 1994ApJS...91..625S I/163 : US Naval Observatory Pleiades Catalog II/131 : Tonantzintla Pleiades Flare Stars (Haro+ 1982) J/ApJS/85/315 : F, G and K dwarf stars of the Pleiades (Soderblom+ 1993) J/A+A/299/696 : Pleiades field Membership probabilities (Schilbach+, 1995) Hambly N.C et al. 1993, A&AS 100, 607 =Cat <J/A+AS/100/607> Haro G. et a. 1982, Bol. Inst. Tonantzintla 3, 3 =Cat <II/131> Hertzsprung E. 1947 Ann. Sternw. Leiden, 19, 1 =1947AnLei..19a...1H Clusters, open X-ray sources open clusters and associations: individual (Pleiades) stars: late-type surveys We have obtained deep ROSAT images of three regions within the Pleiades open cluster. We have detected 317 X-ray sources in these ROSAT PSPC images, 171 of which we associate with certain or probable members of the Pleiades cluster. We detect nearly all Pleiades members with spectral types later than G0 and within 25 arcminutes of our three field centers where our sensitivity is highest. This has allowed us to derive for the first time the luminosity function for the G, K, and M dwarfs of an open cluster without the need to use statistical techniques to account for the presence of upper limits in the data sample. Because of our high X-ray detection frequency down to the faint limit of the optical catalog, we suspect that some of our unidentified X-ray sources are previously unknown, very low-mass members of the Pleiades.
ROSAT
Detected X-ray sources X-ray sources detected between 40' and 50' off-axis NoX X-ray number --- RAh Right ascension (J2000) of the source h RAm Right ascension (J2000) of the source min RAs Right ascension (J2000) of the source s DE- Declination sign --- DEd Declination (J2000) of the source deg DEm Declination (J2000) of the source arcmin DEs Declination (J2000) of the source arcsec Rate1 Centre field rate ct/s e_Rate1 rms uncertainty on Rate1 ct/s Dist1 Center Field distance arcmin Rate2 Northeast Field rate ct/s e_Rate2 rms uncertainty on Rate2 ct/s Dist2 Northeast Field distance arcmin Rate3 Northwest field rate ct/s e_Rate3 rms uncertainty on Rate3 ct/s Dist3 Northwest field distance arcmin Source Optical candidate number=1 HCG numbers are from Haro et al. (1982) <II/131> H II numbers are from Hertzsprung (1947) --- n_Source Note on Source number=2 the letters correspond to the following notes: a: Although the signal-to-noise ratio of this source is below our threshold of 2.5, it was retained after visual inspection of the image b: Star position from Hambly et al. (1993). We have assumed HII 996 is the optical counterpart. c: This source has been identified with Alcyone (HII 1432), the brightest Pleiades at V_0_=2.75. This source may in fact be two sources, with the softer component to the south being closer to Alcyone. d: Star position from Hambly et al. (1993). We have assumed HCG 311 is the optical counterpart. e: Both HII 1797 and HCG 315 are too far from the X-ray centroid to be likely optical counterparts. As a result, upper limits were determined for both these stars. f: Star position from Hambly et al. (1993). We have assumed HCG 327 is the optical counterpart. g: Star position from Hambly et al. (1993). We have assumed HCG 337 is the optical counterpart. h: Hyades cluster member. i: Not a Pleiades cluster member. --- DRA Offset in right ascension arcsec DDE Offset in declination arcsec Source2 Second optical candidate number=1 HCG numbers are from Haro et al. (1982) <II/131> H II numbers are from Hertzsprung (1947) --- n_Source2 Note on Source2 number=2 the letters correspond to the following notes: a: Although the signal-to-noise ratio of this source is below our threshold of 2.5, it was retained after visual inspection of the image b: Star position from Hambly et al. (1993). We have assumed HII 996 is the optical counterpart. c: This source has been identified with Alcyone (HII 1432), the brightest Pleiades at V_0_=2.75. This source may in fact be two sources, with the softer component to the south being closer to Alcyone. d: Star position from Hambly et al. (1993). We have assumed HCG 311 is the optical counterpart. e: Both HII 1797 and HCG 315 are too far from the X-ray centroid to be likely optical counterparts. As a result, upper limits were determined for both these stars. f: Star position from Hambly et al. (1993). We have assumed HCG 327 is the optical counterpart. g: Star position from Hambly et al. (1993). We have assumed HCG 337 is the optical counterpart. h: Hyades cluster member. i: Not a Pleiades cluster member. --- DRA2 Offset in right ascension of Source2 arcsec DDE2 Offset in Declination of Source2 arcsec Source3 Third optical candidate number=1 HCG numbers are from Haro et al. (1982) <II/131> H II numbers are from Hertzsprung (1947) --- DRA3 Offset in right ascension of Source3 arcsec DDE3 Offset in Declination of Source3 arcsec Optical and X-ray data for known Pleiades members NoO Optical catalog index number --- NoX X-ray source number --- Name Star name --- V0 Absolute V magnitude mag (B-V)0 Absolute B-V color index mag (V-I)0 Absolute V-I color index mag l_vsini Limit flag on vsini --- vsini Rotational velocity km/s l_logLX Limit flag on logLX --- logLX X-ray luminosity 10-7W n_logLX v when X-ray emission is variable --- e_logLX rms uncertainty on logLX 10-7W l_log(LX/Lbol) Limit flag on log(LX/Lbol) --- log(LX/Lbol) X-ray luminosity versus bolometric luminosity ratio --- Name2 Other name --- Name3 Other name --- Optical data for known Pleiades members with blended X-ray emission NoO Optical number --- NoX X-ray number --- Name Star name --- n_Name Note on name number=1 a: Blended with HCG 125. See table4 b: Blended with HCG 128. See table4 --- V0 Absolute V magnitude mag (B-V)0 Absolute B-V color index mag (V-I)0 Absolute V-I color index mag l_vsini Limit flag on vsini --- vsini Rotational velocity km/s logLbol Bolometric luminosity 10-7W Name2 Other name --- Name3 Other name --- table2.tex LaTeX version of table2 table3.tex LaTeX version of table3 table7.tex LaTeX version of table7 table8.tex LaTeX version of table8 Patricia Bauer CDS 1996 Aug 14 Marc Gagne <marc@casa.Colorado.EDU> J_ApJS_91_625.xml Ultracompact HII regions II. New high-resolution radio images. J/ApJS/91/659 J/ApJS/91/659 Ultracompact HII regions radio images Ultracompact HII regions II. New high-resolution radio images. S Kurtz E Churchwell D O S Wood Astrophys. J. Suppl. Ser. 91 659 1994 1994ApJS...91..659K J/ApJS/69/831 : 1989ApJS...69..831W : Wood and Churchwell, Paper I H II regions Radio sources HII regions ISM: structure radio continuum: ISM Radio continuum observations were made of 59 IRAS sources that have 100{mu}m flux densities >=1000Jy and far-infrared colors identified with ultracompact (UC) HII regions. Eighty percent were found to have associated compact radio sources. Seventy-five sources were detected at <~1" resolution at 3.6 and 2cm wavelengths, for which we provide contour plots and flux density distributions ranging from the radio to the near-infrared. Over half are unresolved and their morphologies undetermined. The remaining sources can be described by only five morphological classes, whose frequency of occurrence is consistent with that of the Wood and Churchwell survey (1989ApJS...69..831W). We calculate physical properties of the nebulae and show that they are consistent with UC photoionized regions. Alternative explanations are explored and found to be unlikely. The correlation of UC HII region positions with proposed spiral arms is examined and found to be well correlated only for the local spiral arm or "spur". No obvious enhancement of UC HII regions is apparent along the proposed Sagittarius and Scutum arms, probably because of inaccuracies in the kinematic distances. We find the latitude distribution of UC HII regions to lie in the range 0.5deg<[b_FWHM_]<=0.8deg. No correlation between size and density of cometary and core-halo UC HII regions is found, consistent with the bow shock interpretation of these morphologies. Spherical and unresolved UC HII regions, however, appear to show a trend toward lower densities with increasing size, as expected for expanding HII regions. The observed ratios of far-infrared to radio flux densities of UC HII regions lie in the range 10^3^ to >=10^5^. By applying the results of model atmospheres, it is shown that this ratio depends on spectral type, ranging from ~10^3^ for an O4 star to >=10^5^ for a B3 star. We find that many of the UC HII regions in our sample must be excited by a cluster of stars, and most probably contain significant amounts of dust.
Observed Source Parameters Name Radiosource designation --- Mtype Morphological type number=1 We use the following abbreviations for the morphological types: C = cometary CH = core-halo G = Gaussian U = unresolved SH = shell MP = multiply peaked I = irregular --- lambda Observations wavelength (2 or 3.6) cm RAh Source right ascension (1950) number=2 Source positions are accurate to approximately 0.1". We report positions to 0.01" only to aid in the identification of closely spaced components. h RAm Source right ascension (1950) min RAs Source right ascension (1950) s DE- Declination sign --- DEd Source declination (1950) number=2 Source positions are accurate to approximately 0.1". We report positions to 0.01" only to aid in the identification of closely spaced components. deg DEm Source declination (1950) arcmin DEs Source declination (1950) arcsec SPeak Peak flux density (in mJy/beam) mJy SInt Integrated flux density mJy RAbox Integrated box right ascension arcsec DEbox Integrated box declination arcsec Dmax Maximum diameter number=3 Source dimensions are accurate to within approximately 15%. arcsec n_Dmax P: Ponctual source --- Dmin Minimum diameter number=3 Source dimensions are accurate to within approximately 15%. arcsec n_Dmin P: Ponctual source --- Maj Half-power beam width (HPBW) major axis arcsec Min Half-power beam width (HPBW) minor axis arcsec Map Map RMS (in mJy/beam) mJy Note Notes number=4 1: Examination of the 3.6cm map indicates that this source is too large to be imaged at 2cm in the B array. Although the source was detected, no fluxes can be reliably reported. 2: Source is marginally detected at 2cm, observed parameters should be considered approximate. 3: Source has an extended tail to the east. The source sizes reported are for the core region of emission, but the integration boxes for the flux densities include the tail. 4: At 3.6cm this appears as a multiply peaked source. At 2cm it is resolved into two sources, G32.796+0.191 and a cometary source to the north, G32.797+0.191. The 3.6cm flux density is for both sources, but the 2cm flux is for G32.796 only. 5: At 3.6cm this is not resolved from G32.797; a separate 3.6cm flux density cannot be measured. The peak position at 3.6cm is the position quoted for the two sources combined (see note 6). 6: At 3.6cm this is not resolved from G32.796; the peak position and flux at 3.6cm are reported, but a separate integrated flux density cannot be determined. 7: A central core with an extended tail to the north; the flux density and size given here are for the core only. 8: The total flux density of the complex-including the three individual sources and the extended tails-is 2.55 Jy at 3.6cm (10.3"x12.2" integration box) and 2.52 Jy at 2cm (9.1"x12.7" integration box). 9: Field contains both as compact Gaussian component (G43.237-0.046) and an extended irregular source (G43.239 0.049). The integrated flux density for the irregular source was calculated by measuring the total for both, then subtracting the flux density from a Gaussian fit of G43.237-0.046. 10: Sizes and flux densities given are for the central core only. A broad extension to the south of size 7"x4" gives a total integrated flux density of 78.2mJy at 3.6cm and 61.5mJy at 2cm. 11: Due to the large primary-beam correction factor, the 2cm flux density cannot be reliably reported. 12: G28.198-0.150 and G28.200-0.049 are ~7" apart but are plotted separately to emphasize the structure of G28.198-0.150, which is 10-20 times weaker than G28.200-0.049. The structure of G28.198-0.150 varies significantly between 3.6 and 2cm. 13: The 3.6 and 2cm images strongly suggest that more than one ionization source is present. 14: A second source, G35.025+0.350, is detected ~2" to the east, so this field is designated as a complex. The second source is marginally detected, and no flux densities are reported. 15: The wide-field images suggest that this is a compact source embedded in a larger field of emission. 16: This field is designated a complex, since 2 separate sources appear to be present; the angular separation is very small, however. 17: This source is in the Cep A East field. There are numerous weak components in the field which we do not image well with our snapshot observations. For more extensive observational results see Hughes (1988ApJ...333..788H). 18: This is the S 140 complex. Coincidence of radio and IR peaks is not strong: IR peaks are seen without significant radio emission and vice versa. See the references indicated in the flux density distribution (Fig.137) for additional information. 19: This is the DR 21 complex. Large-scale structures have been suppressed by removal of the shortest baselines. We detect a third component in the field at delta 42deg09'03" (see Fig.73) but do not report it as a source. Roelfsema, Goss & Geballe (1989A&A...222..247R) report it as component B. 20: G70.330+1.589 and its eastern companion G70.333+1.586 are both shown in the 3.6cm map (Fig.55); only the former is detected at 2cm (Fig.56). Both of these components are more than 2' from the IRAS position, which is coincident with the K3-50 nebula. G70.330 is component C1, and G70.333 is C2 in both Golley & Scott (1977MNRAS.181..703C) and Harris (1975MNRAS.170..139H). 21: Turner & Matthews (1984ApJ...277..164T) report ~0.1" resolution observations and classify both K3-50 (G70.293+1.600) and component C1 (G70.330+ 1.589) as shell structures. 22: Literature values for the distance to ON1 range from 0.4 to 6.6kpc. A value of 1.4 kpc seems the most popular, but we consider the distance too uncertain to derive parameters. Turner & Matthews (1984ApJ...277..164T) report ~0.1" resolution observations and classify it as a shell morphology. Zheng et al. (1985ApJ...293..522Z) provide a useful map showing the radio continuum overlaid with infrared and H2O and OH maser positions from the literature. 23: The 3.6cm map (Fig.19) suggests a cometary morphology, but the 2cm map (Fig.20) is ambiguous. 24: This source lies on the eastern edge of S252, component C, as reported by Felli, Habing, & Israel (1977A&A....59...43F). 25: Marti, Rodriguez, & Reipurth (1993ApJ...416..208M) have made deep continuum images of this source at 20, 6, 3.6, and 2cm. In their maps the object appears highly elongated and is the central exciting source of a very highly collimated double jet with a total projected extent of 5pc. --- James Marcout, Patricia Bauer CDS 1997 Mar 17 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_91_659.xml Post-asymptotic giant branch evolution of low- to intermediate-mass stars J/ApJS/92/125 J/ApJS/92/125 Post-AGB evolution Post-asymptotic giant branch evolution of low- to intermediate-mass stars E Vassiliadis P R Wood Astrophys. J. Suppl. Ser. 92 125 1994 1994ApJS...92..125V Magellanic Clouds planetary nebulae: general stars: evolution stars: interiors In this paper, we present the results for the post-AGB phases of stellar evolutionary sequences, complete from the main-sequence phase, through the AGB phase, and on into the planetary nebula and white dwarf regimes. Mass loss has been included using an empirical formalism derived from observed mass-loss rates of planetary nebula nuclei available in the literature and from radiation-pressure-driven stellar wind theory. Models are calculated for initial masses 0.89, 0.95, 1.0, 1.5, 2.0, 2.5, 3.5, and 5.0M_{sun}_, and metallicities 0.016, 0.008, 0.004, and 0.001. These abundance and mass values were chosen to allow comparison with Galactic, and Magellanic Cloud planetary nebulae and their nuclei. The post-AGB evolutionary sequences fall into two distinct groups depending on when the planetary nebula nuclei leave the AGB: one group where helium-shell burning is dominant, and the other group where hydrogen-shell burning is dominant. Of the 27 computed sequences: 17 are hydrogen-burners, and 10 are helium-burners. In only five cases was any effort made to control the phase of departure from the AGB. Lower mass models are more likely to leave the AGB burning helium, as the preceding AGB evolution has a mass-loss rate which is greatest immediately prior to a helium-shell flash. The calculations are compared with the large observational database that has developed over recent years for the Large Magellanic Cloud. These calculations will be useful for determining the planetary nebula luminosity function, and for the study of the ultraviolet excess observed in elliptical galaxies.
H-Burning PNN Evolutionary Models He-Burning PNN Evolutionary Models H-Like He-Burning PNN Evolutionary Model M Initial, main-sequence mass solMass Y Y index (always 25) solMass Z Metallicity solMass Time Time. Taken to be zero at log Teff = 4. yr log(Teff) Effective temperature K log(L) Luminosity solLum table.tex LaTeX version of the tables Lee Brotzman ADS 12-May-94, Patricia Bauer CDS 1994 Nov 03 AAS CD-ROM series, Volume 2, 1994 Addresses: Vassiliadis E. Mount Stromlo and Siding Spring Observatories, Institute of Advanced Studies, The Australian National Observatory, Private Bag, Weston Creek P.O., A.C.T. 2611, Australia Wood P.R. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 J_ApJS_92_125.xml A catalog of recent supernovae. J/ApJS/92/219 J/ApJS/92/219 Catalog of recent supernovae A catalog of recent supernovae. S Van den Bergh Astrophys. J. Suppl. Ser. 92 219 1994 1994ApJS...92..219V II/133 : Photoelectric UBV observations of supernovae II/159 : Asiago Supernova Catalogue 1988 II/189 : A catalogue of magnitude observations of type I supernovae II/201 : Sternberg SN Catalogue, 1994Sep. II/205 : GCVS, Vol. V.: Extragalactic Variable Stars Gomez G. & Lopez 1993, AJ 106, 245 (=1993AJ....106..245G) Lauberts, A., 1982 The ESO/Uppsala Survey of the ESO (B) Atlas (Garching: European Southern Observatory) (Catalogue<VII/34B>) Vorontsov-Velyaminov, B.A., et al. Morphological Catalogue of Galaxies I-IV MCG (Moscow: Moscow University) 1962-1974 (Catalogue<VII/62A>) Pennypacker et al. 1992, IAUC 5652 (=1992IAUC.5652....1P) Sandage, A., & Tammann, G.A. 1981 A Revised Shapley-Ames Catalog at Bright Galaxies (Washington: Carnegie Institution) (Catalogue<VII/51>) Schmidt B.P., et al. 1993 AJ 105, 2236 (=1993AJ....105.2236S) de Vaucouleurs, G., de Vaucouleurs, A., Corwin, H.G., Buta, R.J., Paturel, G., & Fouque, P. 1991 Third Reference Catalogue of Bright Galaxies (RC3) (Berlin: Springer) (Catalogue<VII/155>) Supernovae supernovae: general A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.
Data on recent supernova SN Supernova name --- n_SN A 'N' indicates that it is not a supernova --- Gal Parent galaxy name number=1 N = NGC, I = IC, U = UGC. The letters E and M indicate that the galaxy is listed in the ESO (Lauberts 1982) or MCG (Vorontsov-Velyaminov et al. 1962-1974) Catalogs, respectively --- MType Parent galaxy classification types number=2 Galaxy classification types were, in order of preference, drawn from (a) Sandage and Tammann (1981) (Catalogue <VII/51>) (b) an unpublished catalog of DDO classifications by the present author (c) de Vaucouleurs et al. (1991) (RC3, Catalogue <VII/155>) (d) Lauberts (1982) (Catalogue <VII/34B>) --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec RV Radial velocity number=3 Galaxy radial velocity, preferentially drawn from the optical heliocentric listing of de Vaucouleurs et al. (1991) km/s Mag Discovered magnitude mag n_Mag Color of discovered magnitude number=4 Both mpg, blue and B are called B, MJ is designated J, mpv and V are both indicated by V, r and R are both called as R. For a few supernovae I or K discovery magnitudes are listed --- IAUC Number of IAU Circular giving discovery information --- Offsets Offsets from nucleus of galaxy --- Type Supernova type --- IAUC(SN) Number of IAU Circular from which SN type was drawn --- Notes Remarks on some individual supernovae number=5 individual notes: 1 Offset from nucleus given as 25" NE in IAU Circular 4758. 2 Offsets provided by Tsvetkov et al. 3 Offset from nucleus given as 5.8" SW in IAUC 5046. 4 According to IAUC 4959 this is a compact HII region, not a supernova 5 Type II-P supernova according to Schmidt et al. (1993). 6 IAUC 5111 gives type Ib, whereas IAUC 5129 assigns a type Ic. 7 Located between two galaxies. Quoted position is that of the supernova. 8 Not a supernova according to IAUC 5270. 9 Quasar according to IAUC 5328. 10 The "anonymous" galaxy in IAUC 5356 is, in fact, MCG 4-6-29. 11 It is not clear whether the position quoted in IAUC 5446 refers to the galaxy or to the supernovae. 12 According to IAUC 5468 possibly a subluminous SNIa like SN1991bg. 13 Foreground M star according to IAUC 5528. 14 Occurred 4"N of SN 1992R (Gomez & Lopez 1993). 15 Supernova located 45" from nucleus. 16 On the basis of photometry Pennypacker et al. (IAUC 5652) claim that this supernova was probably of type Ia. --- Ages of supernova at discovery SN Supernova name --- Gal Parent galaxy name --- Type Type of the supernova --- Age Information on the spectral age --- l_T Limit flag on T --- T Evolutionary age at the time of the discovery d u_T Uncertainty flag on T --- e_T rms uncertainty on T d Patricia Bauer CDS 1996 May 14 Sidney van den Bergh <vdb@dao.nrc.ca> J_ApJS_92_219.xml The Einstein database of IPC X-ray observations of optically selected and radio-selected quasars. I. J/ApJS/92/53 J/ApJS/92/53 Einstein database of quasars. I. The Einstein database of IPC X-ray observations of optically selected and radio-selected quasars. I. B Wilkes H Tananbaum D M Worrall Y Avni M S Oey J Flanagan Astrophys. J. Suppl. Ser. 92 53 1994 1994ApJS...92...53W galaxies: Seyfert quasars: general X-rays: galaxies We present the first volume of the Einstein quasar database. The database includes estimates of the X-ray count rates, fluxes, and luminosities for 514 quasars and Seyfert 1 galaxies observed with the Imaging Proportional Counter (IPC) aboard the Einstein Observatory. All were previously known optically selected or radio-selected objects, and most were targets of the X-ray observations. The X-ray properties of the AGNs have been derived by reanalyzing the IPC data in a systematic manner to provide a uniform database for general use by the astronomical community. We use the database to extend earlier quasar luminosity studies which were made using only a subset of the currently available data. The database can be accessed on Internet via the SAO Einstein on-line system ("Einline") and is available in ASCII format on magnetic tape and DOS diskette.
Einstein
Quasars and Seyfert 1 galaxies included in database Name Coordinate-based designation --- Other Other common names --- RAh Right ascension B1950 h RAm Right ascension B1950 min RAs Right ascension B1950 s DE- Declination sign --- DEd Declination B1950 deg DEm Declination B1950 arcmin DEs Declination B1950 arcsec Ref Reference number=1 References ANDP Anderson,S. 1990, private communication BREG Bregman,J.N., Glassgold,A.E., Huggins,P.J., and Kinney, A.L. 1985, ApJ, 291, 505 (and references therein) B2 Colla,G. et al, 1970, A&AS, 1, 281 GSL86 Green,R.F., Schmidt,M., and Liebert,J. 1986, ApJS, 61, 305 HB89 Hewitt,A. and Burbidge,G. 1989, ApJS, 69,1 (Information extracted from computer tapes and includes all data from Hewitt and Burbidge, 1987) SG83 Schmidt,M. and Green,R.F. 1983, ApJ, 269, 352 V87 Veron-Cetty,M.-P. and Veron,P. 1987 (Information extracted from computer tapes and includes all data in ESO Scientific Report No. 5) --- z Redshift --- Notes Coded notes number=2 1 Object included in optically selected sample for further analysis. 2 z from Marshall et al, 1984 and differs slightly from HB89. 3 Included in optically selected sample due to independent selection in prism survey (not flagged as ``O'' or ``C'' in HB89). 4 Not included in PG ``X-ray Sample'' since it falls in declination zone generally not observed. 5 Redshift and optical magnitude (see Table 6) from Sramek and Weedman (1980) and differs from HB89 due to transcription error passed through intermediate references. --- Sample Indication of complete subsample number=3 As a whole the sample is incomplete, although it contains a few complete subsamples: PG 64 PG quasars (Tananbaum et al. 1986, ApJ, 305, 57) 3CR 33 3CR radio quasars (Tananbaum et al. 1983, ApJ, 268, 60) BF 30 Braccesi BF quasars (Marshall et al. 1984, ApJ, 283, 50) --- Einstein observational details Name Coordinate-based designation --- m_Name Multiplicity index on name --- Seq Unique Einstein observation sequence number --- Note Coded note number=1 1 Data set used in subsequent analysis when multiple X-ray observations exist 2 Special Processing due to obscuration, 1/2 circle 3 Special Processing due to obscuration, 3/4 circle 4 Not target 5 X-ray position > 1' from optical 6 Net counts unreliable 7 Special processing for nearby contaminating source 8 TON 156 is ~30'' away; flux upper limit for TON 155 calculated first due to closer positional agreement with potential IPC source 9 Marginal detection: >3 sigma in detection process, but net counts in circle less than 3 times the uncertainty in this quantity 10 <3 sigma detection if Poisson statistics are used --- Start Date for start of observation --- End Date for end of observation --- Counts Net source counts --- e_Counts rms uncertainty on Counts --- Live Live Time s Angle Off-axis angle arcmin Gain Gain --- Fluxes and luminosities for energy index of 0.0 Name Coordinate-based designation --- m_Name Multiplicity index on name --- Seq Unique Einstein observation sequence number --- N(H) Galactic N(H) value cm-2 Note Coded note number=1 1 N_H from Heiles, C. and Cleary, M.N. 1979, Aust. J. Phys. Astrophys. Suppl., 47, 1. 2 N_H from Harris, D. et al., Einstein Observatory Source Catalogue, 1993, NASA publication (in press). 3 Positive (>3 sigma) source detection with best estimate of count rate (and flux and luminosity) less than three times the associated uncertainty. --- l_FDa Limit flag on flux density --- FDa Flux density (1keV) mW/m2/Hz l_Fa Limit flag on flux --- Fa Flux (0.16-3.5 keV) mW/m2 l_La Limit flag on luminosity --- La Luminosity (0.2-4.5 keV) 10-7W l_LDa Limit flag on luminosity density --- LDa Luminosity density 10-7W/Hz Fluxes and luminosities for energy indices of 0.5 and 1.0 Name Coordinate-based designation --- m_Name Multiplicity index on name --- Seq Unique Einstein observation sequence number --- l_FDb Limit flag on FDb --- FDb Flux density (1keV; index 0.5) mW/m2/Hz l_Fb Limit flag on Fb --- Fb Flux (0.16-3.5 keV; index 0.5) mW/m2 l_Lb Limit flag on Lb --- Lb Luminosity (0.2-4.5 keV; index 0.5) 10-7W l_LDb Limit flag on LDb --- LDb Luminosity density (2keV; index 0.5) 10-7W/Hz l_FDc Limit flag on FDc --- FDc Flux density (1keV; index 1.0) mW/m2/Hz l_Fc Limit flag on Fc --- Fc Flux (0.16-3.5 keV; index 1.0) mW/m2 l_Lc Limit flag on Lc --- Lc Luminosity (0.2-4.5 keV; index 1.0) 10-7W l_LDc Limit flag on LDc --- LDc Luminosity density (2keV; index 1.0) 10-7W/Hz Fluxes and luminosities for energy indices of 1.5 and 2.0 Name Coordinate-based designation --- m_Name Multiplicity index on name --- Seq Unique Einstein observation sequence number --- l_FDd Limit flag on FDd --- FDd Flux density (1keV; index 1.5) mW/m2/Hz l_Fd Limit flag on Fd --- Fd Flux (0.16-3.5 keV; index 1.5) mW/m2 l_Ld Limit flag on Ld --- Ld Luminosity (0.2-4.5 keV; index 1.5) 10-7W l_LDd Limit flag on LDd --- LDd Luminosity density (2keV; index 1.5) 10-7W/Hz l_FDe Limit flag on FDe --- FDe Flux density (1keV; index 2.0) mW/m2/Hz l_Fe Limit flag on Fe --- Fe Flux (0.16-3.5 keV; index 2.0) mW/m2 l_Le Limit flag on Le --- Le Luminosity (0.2-4.5 keV; index 2.0) 10-7W l_LDe Limit flag on LDe --- LDe Luminosity density (2keV; index 2.0) 10-7W/Hz Objects not included in this paper Objects included in this paper, with incomplete analysis for individual observations listed here Name Coordinate-based designation --- m_Name Multiplicity index on name --- Seq Unique Einstein observation sequence number --- Note Explanation --- Optical data Name Coordinate-based designation --- m_Name Multiplicity index on name --- Seq Unique Einstein observation sequence number --- Bmag Optical B magnitude --- n_Bmag Note on B number=1 1 Data used in subsequent analysis when multiple X-ray observations exist. 2 Magnitude quoted as V in HB89 or VV87, but taken as B in this paper on basis of original references. 3 Two observations of same quasar in two different X-ray fields lead to slightly different N 's and thereby slightly different optical extinctions and optical luminosities. 4 VV87 computer tapes or HB89 computer tapes give magnitude update relative to hard copy catalog. 5 B magnitude from Hoag and Smith (1977) as referenced in HB89. 6 B magnitude from Burbidge and Strittmatter (1972) as referenced in HB89. 7 B magnitude from Kristian and Sandage (1970) as referenced in VV87. 8 B and V magnitudes from Usher (1978) as referenced in HB89. 9 B magnitude from Willis and de Ruiter (1977) as referenced in VV87. 10 B magnitude from Vaucher and Weedman (1980) as referenced in HB89. 11 B magnitude from Cohen et al. (1977) as referenced in VV87. 12 B magnitude from Peterson, Bolton, and Shimmins (1973) as referenced in HB89. 13 B and V magnitudes from Rafanelli and Schulz (1983) as referenced in VV87. 14 Original reference quotes magnitude as R; taken as V here due to lack of additional data. 15 No published data (other than HB89) found to verify magnitude or band; HB89 value taken as V magnitude. 16 V magnitude from Hunstead, Murdoch, and Shabbrook (1978) as referenced in HB89. 17 B and V magnitudes from Usher (1981) as referenced in HB89. 18 B and V magnitudes from Formiggini et al. (1980) as referenced in HB89. 19 B magnitude from Marshall et al. (1984) as referenced in HB89. 20 B magnitude from Braccesi et al. (1970) as referenced in HB89. 21 B magnitude from Veron et al. (1976) as referenced in HB89. --- r_Bmag B reference number=2 ANDP Anderson, A. 1990, private communication H92 Hazard, C. 1992, private communication HB89 Hewitt, A. and Burbidge, G. 1989, ApJS, 69, 1 SG83 Schmidt, M. and Green, R.F. 1983, ApJ, 269, 352 SIMBA SIMBAD on-line catalogue SW80 Sramek, R. and Weedman, D. 1980, ApJ, 238, 435 VV87 Veron-Cetty, M.-P. and Veron, P. 1987 ESO Scientific Report No. 5 --- Vmag Optical V magnitude mag r_Vmag V reference number=2 ANDP Anderson, A. 1990, private communication H92 Hazard, C. 1992, private communication HB89 Hewitt, A. and Burbidge, G. 1989, ApJS, 69, 1 SG83 Schmidt, M. and Green, R.F. 1983, ApJ, 269, 352 SIMBA SIMBAD on-line catalogue SW80 Sramek, R. and Weedman, D. 1980, ApJ, 238, 435 VV87 Veron-Cetty, M.-P. and Veron, P. 1987 ESO Scientific Report No. 5 --- L(opt) Spectral luminosity at 2500 A 10-7W/Hz l_alpha Limit flag on Alpha --- alpha Effective optical-to-X-ray power-law slope --- Lee Brotzman ADS 12-May-94 Patricia Bauer CDS 1994 Oct 28 AAS CD-ROM series, Volume 2, 1994 Addresses: Wilkes B. wilkes@cfa.harvard.edu Tananbaum H. ht@cfa.harvard.edu Worrall D.M. dmw@cfa.harvard.edu Flanagan J. Harvard/Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138 Avni Y. Harvard/Smithsonian Center for Astrophysics, Deceased Oey M.S. oey@as.arizona.edu Steward Observatory, Tucson, AZ 85721 J_ApJS_92_53.xml A Sensitive 1.5 GHz radio survey around the north ecliptic pole J/ApJS/93/145 J/ApJS/93/145 Radio survey around north ecliptic pole A Sensitive 1.5 GHz radio survey around the north ecliptic pole R I Kollgaard W Brinkmann M M Chester E D Feigelson P Hertz P Reich R Wielebinski Astrophys. J. Suppl. Ser. 93 145 1994 1994ApJS...93..145K Radio sources catalogs radio continuum: general surveys X-rays: general A 29.3deg^2 region surrounding the north ecliptic pole (NEP; R.A.=18h00m, Dec.=+66d30m) was mapped with the Very Large Array at 1.5GHz to support the deepest portion of the ROSAT all-sky soft X-ray survey. The resulting VLA-NEP survey catalog contains 2435 radio sources with flux densities in the range of 0.3-1000mJy, including over 200 fainter than 1mJy. The 28 fields of the inner 1.5deg have noise levels sigma ~=60uJy, and the 85 fields centered between 1.5deg and 3.0deg from the NEP have sigma ~=120uJy. The typical spatial resolution is 20" HPBW, and most positions are accurate to <2". Approximately 6% of the sources are found to be extended with size >30". We have compared the VLA-NEP catalog with four other radio catalogs made at lower resolution, as well as with the NASA Extragalactic Database and find counterparts for ~18% of the VLA-NEP objects. The normalized, differential radio source count is in agreement with the previous studies. Between 1 and 150mJy the slope of the logN-logS relation is 0.68+/-0.03.
VLA-NEP source catalog Name VLA-NEP source name (J2000) --- Field VLA-NEP field designation --- RAh Right Ascension, J2000 (corrected) h RAm Right Ascension, J2000 (corrected) min RAs Right Ascension, J2000 (corrected) s DE- Declination sign --- DEd Declination, J2000 deg DEm Declination, J2000 arcmin DEs Declination, J2000 arcsec e(Pos) Net positional uncertainty arcsec Dis Distance of the source from the field center arcmin Stot Corrected integrated flux density mJy e_Stot rms uncertainty on Stot mJy Speak Corrected peak flux density mJy e_Speak rms uncertainty on Speak mJy SNR Signal-to-noise ratio of the detection --- ID 'ID'= identification listed in table 3 --- Note Additional notes number=1 S = suspect source which lies on an image processing artifact D = double source, either a blend of two comparable sources or two resolved peaks with a common envelope D?= possible double whose features appear at less than 8 x sigma E = extended source, either an elongated source or an object with an asymmetric or complex shape E?= possible extended source, whose features appear at less than 8 x sigma Also included is the angular separation (arcminutes) between the peaks of double sources, the angular size of extended sources (measured from the peak to the most distant feature, minus a slight resolution correction), and the position angle (degrees) measured from the brightest peak. --- VLA-NEP sources with possible identifications Name VLA-NEP source, see table 2, field ID --- Flux VLA-NEP total flux density mJy BWE91 BWE91 name number=1 BWE91: Name of any 5 GHz counterpart from Becker, White & Edwards =1991ApJS...75....1B (Catalog <VIII/13>) --- SBWE91 BWE91 catalogued flux density mJy LRW88 LRW88 name number=2 LRW88: Name of any 2.7 GHz Effelsberg counterpart from Loiseau et al. =1988A&AS...75...67L --- SLRW88 LRW88 catalogued flux density mJy WB92 WB92 name number=3 WB92: Name of any 1.4 GHz counterpart from White & Becker 1992, =1992ApJS...79..331W (Catalog <VIII/17>) --- SWB92 WB92 catalogued flux density mJy LRW92 LRW92 name number=4 LRW92: Name of any 8C counterpart from Lacy, Rawlings & Warner 1992, =1992MNRAS.256..404L --- NED NASA Extragalactic Database name number=5 NED: Name of any NASA Extragalactic Database counterpart that is not from the four previous surveys --- Vned NED visual magnitude mag SI1 Spectral index between 1.5GHz and 5GHz --- SI2 Spectral index between 1.5GHz and 2.7GHz --- Ref Reference number number=6 Reference number for sources with information from NED 1 Lacy, Rawlings, & Warner =1992MNRAS.256..404L 2 Zwicky & Herzog 1968, Catalogue of Galaxies and Clusters of Galaxies (Pasadena: California Institute of Technology) (Catalog <VII/49>) 3 Joint IRAS Science Working Group 1988, Infrared Astronomical Satellite Catalogs, The Point Source Catalog (ver. 2) (NASA RP-1190) (Catalog <II/125>) 4 Kojoian et al. =1981AJ.....86..820K 5 Moshir et al 1990, Infrared Astronomical Catalogs, The Faint Source Catalog (ver. 2) (Catalog <II/156>) 6 Ashby, Houck, & Hacking =1992AJ....104..980A 7 Nilson 1973, Uppsala General Catalogue of Galaxies, Acta Universitatis Upsalienis, Nava Regiae Societatis Upsaliensis, Series V: vol. 1 (Catalog <VII/26>) 8 Abell, Corwin, & Olowin =1989ApJS...70....1A (Catalog <VII/110>) 9 Vorontsov-Velyaminov & Krasnogorskaja 1962, Morphological Catalogue of Galaxies (Moscow: Moscow State University) (Catalogs <VII/62> and <VII/100>) 10 Sovers et al. =1988AJ.....95.1647S 11 Clements 1983 =1983MNRAS.204..811C 12 Dressel & Condon 1976, ApJS, 31, 187 13 Takase & Miyauchi-Isobe 1989, Pub. Nat. Astr. Ast. Obs. Japan, =1989PNAOJ...1...97T 14 Russell et al. =1990AJ.....99.2059R (Guide Star Catalog) 15 Burg et al. =1992A&A...259L...9B 16 Zwicky 1971, Catalogue of Selected Compact Galaxies and Post-Eruptive Galaxies (Zurich: Offsetdruck L. Speich) 17 Tsvetkov & Bartunov 1993, Bull Inf. Centre Donnes Stellaires, =1993BICDS..42...17T --- Lee Brotzman ADS 10-Oct-94 Patricia Bauer CDS 1995 Feb 16 AAS CD-ROM series, Volume 3, 1995 Addresses: Kollgaard R.I. <rik@astro.psu.edu> McMath Chester M. <chester@astro.psu.edu> Feigelson E.D. <edf@Feigelson> Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 Brinkmann W. <wpb@ibma.ipp-garching.mpg.de> Max-Planck-Institut fur Extraterrstrische Physik, Giessenbach strasse, 85740 Garching, Germany Hertz P. <hertz@xip.nrl.navy.mil> E.O. Hulburt Center for Space Research, Naval Research Laboratory, Code 7621.5, Washinton, DC 20375-5352 Reich P. <p395pat@mpifr-bonn.mpg.de> Wielebinski R. <rwielebinski@mpifrbonn.mpg.de> Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany J_ApJS_93_145.xml The galactic open cluster NGC 7419 and its five red supergiants. J/ApJS/93/187 J/ApJS/93/187 UBV Photometry in NGC 7419 The galactic open cluster NGC 7419 and its five red supergiants. A Beauchamp A F J Moffat L Drissen Astrophys. J. Suppl. Ser. 93 187 1994 1994ApJS...93..187B Clusters, open Photometry, CCD open clusters and associations: individual (NGC 7419) stars: evolution supergiants UBV CCD photometry has been carried out on the heavily reddened (A_V_=6.7) Cepheus open cluster NGC 7419. An age of 14+/-2 million yr and a distance of 2.3kpc have been derived using the isochrones of Maeder. The mass function of the cluster satisfies the Salpeter from n(M)~M^-{gamma}^ with {gamma}=2.25. The cluster is dynamically relaxed.
NGC 7419 C 2252+605 22 54.3 +60 50
Coordinates and mean magnitudes of the 518 stars in NGC 7419 with measured V and B magnitudes ID Identification number --- Xpos X coordinate number=1 1 pix = 0.48", positive from right to left, and from bottom to top. pix Ypos Y coordinate number=1 1 pix = 0.48", positive from right to left, and from bottom to top. pix Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag Umag U magnitude mag e_Umag rms uncertainty on Umag mag table1.tex TeX version of table1 Patricia Bauer CDS 1996 Sep 06 Alain Beauchamp <beaucham@ASTRO.UMontreal.ca> J_ApJS_93_187.xml An IUE survey of interstellar H I Ly{alpha} absorption. I. Column densities. J/ApJS/93/211 J/ApJS/93/211 IUE survey of H I Ly{alpha} absorption. I. An IUE survey of interstellar H I Ly{alpha} absorption. I. Column densities. A Diplas B D Savage Astrophys. J. Suppl. Ser. 93 211 1994 1994ApJS...93..211D J/ApJ/427/274 : 1994ApJ...427..274D : Paper II. Diplas & Savage, (1994) H I data Photometry, UBV Redshifts Ultraviolet ISM: abundances stars: early-type ultraviolet: ISM We measure Galactic interstellar neutral hydrogen column densities by analyzing archival interstellar Ly{alpha} absorption line data toward 554 B2 and hotter stars observed at high resolution with the IUE satellite. This study more than doubles the number of lines of sight with measures of N(H I) based on Ly{alpha}. We have included the scattered light background correction algorithm of Bianchi and Bohlin (1984A&A...134...31B) in our data reduction. We use the correlation between the Balmer discontinuity [c_1_] index and the stellar Ly{alpha} absorption in order to assess the effects of stellar Ly alpha contamination. Approximately 40% of the B stars with measured [c_1_] index, exhibit serious stellar Ly{alpha} contamination. Table 1 contains the derived values of the interstellar N(H I) for 393 stars with at most small amounts of stellar contamination. Table 2 lists the observed values of total N(H I) for 161 stars with suspected stellar Ly alpha contamination and/or uncertain stellar parameters.
IUE
Interstellar atomic hydrogen column densities Atomic hydrogen column densities for stars with suspected stellar Lyman-alpha contamination and/or uncertain stellar parameters HD/BD HD or BD star name --- Name Other name --- GLON Galactic longitude deg GLAT Galactic latitude deg SpType Spectral type --- Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag --- B-V B-V colour index mag E(B-V) B-V colour excess mag E2175 2175A Bump strength measure mag r Adopted distance pc z Stellar distance above or below the Galactic plane pc log(N(HI)) Observed HI density column cm-2 e_log(N(HI)) rms uncertainty on log(N(HI)) cm-2 [c1] Stroemgren Balmer jump index corrected for for extinction ([c1]=c1-0.2(b-y)) --- log(N(HI))s Stellar HI density column when [c1] available cm-2 log(N(HI))i Interstellar HI density column corrected for stellar absorption cm-2 Ref Reference number=1 References are: (1) Walborn, 1972AJ.....77..312W (2) Walborn, 1973AJ.....78.1067W (3) Walborn, 1971ApJS...23..257W (4) Lesh, 1968ApJS...17..371L (5) Lesh, 1972A&AS....5..129L (6) Garrison et al., 1977ApJS...35..111G (7) Hill, 1970MNRAS.150...23H (8) Morgan et al., 1955ApJS....2...41M (9) Kilkenny, 1987MNRAS.228..713K (10) Dworetsky et al., 1982MNRAS.201..901D (11) Garmany et al., 1982ApJ...263..777G (12) Hiltner et al., 1969ApJ...157..313H (13) Hill et al., 1974MNRAS.168..451H (14) Mathys, 1989A&AS...81..237M (15) Humphreys, 1978ApJS...38..309H (16) Walborn et al., 1985NASAR1155....0W (Cat. <III/115>) (17) Tobin, 1985A&AS...60..459T (18) Conti et al., 1983ApJ...274..302C (19) Kilkenny et al., 1975MNRAS.171..353K (20) Nicolet, 1978A&AS...34....1N (21) Crawford et al., 1971AJ.....76.1058C (22) Hoffleit, 1964, Bright Star Catalogue, See Cat. <V/50> (23) Bohlin et al., 1978ApJ...224..132B (24) Mathys, 1988A&AS...76..427M (25) Johnson et al., 1956ApJ...123..267J (26) Sharpless, 1952ApJ...116..251S (27) Schild & Chaffe, 1971ApJ...169..529S (30) Conti & Alschuler, 1971ApJ...170..325C (31) Conti & Leep, 1974ApJ...193..113C (32) Turner, 1976ApJ...210...65T (33) Walborn, 1982AJ.....87.1300W (34) Simonson, 1968ApJ...154..923S (35) Weber et al., 1971ApJ...166..543W (36) Sembach & Savage, 1992ApJS...83..147S (37) Edgar & Savage, 1989ApJ...340..762E (38) Schild et al., 1969ApJ...156..609S (39) Sembach, Savage, & Massa, 1991ApJ...372...81S (40) Kilkenny, 1977MNRAS.181..611K (41) Buscombe, 1980, MK Spectral Classification, See Cat. <III/189> (42) Blanco et al., 1968PUSNO..21.....B (43) Walborn et al., 1990PASP..102..543W (44) Garrison, 1970AJ.....75.1001G (45) Wesselius et al., 1982A&AS...49..427W (46) Kennedy & Buscombe 1974, MK Spectral Class., See Cat. <III/78> (47) Tobin & Kilkenny, 1981MNRAS.194..937T (48) Houk & Cowley, 1975MSS...C01....0H (Cat. <III/31>) (49) Buscombe, 1977, MK Spectral Classification, See Cat. <III/189> (50) Houk & Smith-Moore, 1988MSS...C04....0H (51) Thackeray & Andrews, 1974A&AS...16..323T (52) Gutierrez-Moreno & Moreno, 1968ApJS...15..459G (53) Morris, 1961MNRAS.122..325M (54) van der Hucht et al., 1981SSRv...28..227V (55) Crawford et al., 1973AJ.....78..738C (56) Houk, 1982MSS...C03....0H (57) Walker, 1956ApJS....2..365W (58) Guetter, 1968PASP...80..197G (59) Kilkenny, 1984MNRAS.211..969K (60) Kilkenny et al., 1988SAAOC..12....1K (61) Boggs & Bohm-Vitense, 1989ApJ...339..209B (62) Chini & Neckel, 1981A&A...102..171C (63) Heber et al., 1988A&A...194..223H (64) Maciel & Pottasch, 1980A&A....88....1M (65) Downes, 1986ApJS...61..569D (66) Heap, 1977ApJ...215..609H (67) Kilkenny,, 981MNRAS.194..927K --- James Marcout, Patricia Bauer CDS 1997 Jan 28 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_93_211.xml Supplement to the Arecibo 1612 MHz survey of color-selected IRAS sources J/ApJS/93/549 J/ApJS/93/549 Arecibo 1612 MHz survey supplement Supplement to the Arecibo 1612 MHz survey of color-selected IRAS sources B M Lewis Astrophys. J. Suppl. Ser. 93 549 1994 1994ApJS...93..549L II/125 : IRAS Point Source Catalogue, Version 2.0 (IPAC 1986) J/A+AS/90/327 : IRAS Point Source 1612MHz OH survey (te Lintel Hekkert+ 1991) J/ApJS/89/189 : IRAS PSC new OH/IR stars. III. (Chengalur+ 1993) Eder et al., New OH/IR stars from IRAS sources. I. =1988ApJS...66..183E Lewis et al., New OH/IR stars from IRAS sources. II. =1990ApJ...362..634L Changalur et al., New OH/IR stars from IRAS sources. III. =1993ApJS...89..189C Radio sources infrared: stars radio lines: stars stars: AGB and post-AGB surveys The completeness of the Arecibo 1612 MHz survey of color-selected/IRAS sources (see references) is extended to (25-12){mu}m>-0.7. In addition (1) most IR sources with spectral types normally associated with OH/IR stars and colors outside the coverage of the original survey have been examined; (2) most ambiguous observations during the survey have been reobserved: (3) most single peaked sources have been reexamined, and 17 found with second peaks. We report 39 new 1612MHz detections, of which 34 are original. These are also surveyed in the mainlines. Analysis of the complete flux-limited survey confirms the existence of a longitude sensitivity effect in the detection of sources, which reduces the total number detected by ~4%. This analysis sets an upper limit of 16%, on the proportion of a color-selected sample that may be identified with carbon stars and/or star-formation regions.
IRAS
Profile parameters for 1612 MHz detections IRAS IRAS name --- n_IRAS *: part of color-selected Arecibo sample --- Note s: single to double peaked profiles --- GLON Galactic longitude deg GLAT Galactic latitude deg RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec S1612MHz Total integrated 1612MHz flux mJy.km/s S1612-l Integrated 1612MHz flux in the low-velocity half of the spectrum mJy.km/s S1612-h Integrated 1612MHz flux in the high-velocity half of the spectrum mJy.km/s DV100 Velocity separation between the half-power points of the two peaks in the line profile {DELTA}V_100_ km/s u_DV100 Uncertainty flag on DV100 --- DV50 Velocity separation between the half-power points of the two peaks in the line profile {DELTA}V_50_ km/s u_DV50 Uncertainty flag on DV50 --- Vl LSR velocity of the low-velocity peak km/s Vh LSR velocity of the high-velocity peak km/s <V> Systemic LSR velocity km/s (25-12) (25-12){mu}m infrared colour number=1 (25-12)um = log{S(25*12*0.89/S(12)*25*1.09} (60-25)um = log{S(60)*25*0.82/S(25)*60*0.89} mag (60-25) (60-25){mu}m infrared colour number=1 (25-12)um = log{S(25*12*0.89/S(12)*25*1.09} (60-25)um = log{S(60)*25*0.82/S(25)*60*0.89} mag LRS IRAS low-resolution spectral-type --- Name Other name --- IRAS sources without 1612 MHz emission n_IRAS * : part of flux-limited Arecibo sample --- IRAS IRAS name --- GLON Galactic longitude deg GLAT Galactic latitude deg (12-25) (12-25){mu}m infrared color mag (60-25) (60-25){mu}m infrared color mag Main line parameters of 1612 MHz detections IRAS IRAS name number=1 IRAS 19114+0002, 19142+1034, 19246+1637, and 20406+2953 previously detected, the remaining 1612 MHz detections are mainline non detections. --- Sp1667 1667 MHz first peak flux mJy n_Sp1667 Note on Sp1667 number=2 s: the Sp value is sigma value n: not analyzed ): uncertainty flag --- Vp1667 1667 MHz first peak velocity km/s Sp1667b 1667 MHz second peak flux mJy Vp1667b 1667 MHz second peak velocity km/s Sp1665 1665 MHz first peak velocity mJy n_Sp1665 Note on Sp1665 number=2 s: the Sp value is sigma value n: not analyzed ): uncertainty flag --- Vp1665 1665 MHz first peak velocity km/s u_Vp1665 Uncertainty flag on Vp1665 --- Sp1665b 1665 MHz second peak flux mJy n_Sp1665b Note on Sp1665b number=2 s: the Sp value is sigma value n: not analyzed ): uncertainty flag --- Vp1665b 1665 MHz second peak velocity km/s James Marcout, Patricia Bauer CDS 1997 Mar 20 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_93_549.xml The first Extreme Ultraviolet Explorer source catalog J/ApJS/93/569 J/ApJS/93/569 First EUVE source catalogue The first Extreme Ultraviolet Explorer source catalog S Bowyer R Lieu M Lampton J Lewis X Wu J J Drake R F Malina Astrophys. J. Suppl. Ser. 93 569 1994 1994ApJS...93..569B catalogs ultraviolet: stars The Extreme Ultraviolet Explorer(EUVE) has conducted an all-sky survey to locate and identify point source of emission in four extreme ultraviolet wavelength bands centered at ~100, 200, 400, and 600A. A companion deep survey of a strip along half the ecliptic plane was simultaneously conducted. In this catalog we report the sources found in these surveys using rigorously defined criteria uniformly applied to the data set. These are the surveys to be made in the three longer wavelength bands, and a substantial number of sources were detected in these bands.
EUVE All-Sky Survey EUVE Deep Survey Name Source catalogue number --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin C100 Count rate for 100A band ct/s e_C100 rms uncertainty on C100 ct/s C200 Count rate for 200A band ct/s e_C200 rms uncertainty on C200 ct/s C400 Count rate for 400A band ct/s e_C400 rms uncertainty on C400 ct/s C600 Count rate for 600A band ct/s e_C600 rms uncertainty on C600 ct/s Q Quality factor number=1 Quality factor: 1: probable, 2: possible, U: possible UV leak --- ID1 First identification name --- ID2 Second identification name --- Sp Spectral type of best ID --- Vmag V and B magnitude of best ID mag n_Vmag A '?' indicates unknown magnitude --- Sep Separation between EUV and probable ID arcsec Com Comments number=2 RE: ROSAT WFC catalog (Pounds et al. 1993) 4U: 4th Uhuru catalog (Forman et al. 1978) TD-1: TD-1 survey (Carnochan & Wilson 1983) 1E: first Einstein survey (Giacconi et al. 1979) LTT: Luyten 1957, 1961 NO ID: no identification *: 100 A band count rate is a probable UV leak In table2, number symbol (#) indicates sources also appears in table1. --- Other EUV sources detected by EUVE Name Catalog number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin C100 Count rate 100 A band, all sky survey ct/s e_C100 rms uncertainty on C100 ct/s C200 Count rate 200 A band, all sky survey ct/s e_C200 rms uncertainty on C200 ct/s C400 Count rate 400 A band, all sky survey ct/s e_C400 rms uncertainty on C400 ct/s C600 Count rate 600 A band, all sky survey ct/s e_C600 rms uncertainty on C600 ct/s C100d Count rate 100 A band, deep survey ct/s e_C100d rms uncertainty on C100d ct/s C200d Count rate 200 A band, deep survey ct/s e_C200d rms uncertainty on C200d ct/s ID1 ID name 1 --- Sp Spectral type of ID --- Comment Comments for EUV source number=1 RE = ROSAT WFC catalog (Pounds et al. 1993) 4U = 4th Uhuru catalog (Forman et al. 1978) TD1 = TD1 survey (Carnochan & Wilson 1983) 1E = 1st Einstein survey (Giacconi et al. 1979) LTT = Luyten 1957, 1961 --- Marie-Jose Wagner, Patricia Bauer CDS 1994 Dec 07 UNKNOWN UNKNOWN Keypunched at CDS J_ApJS_93_569.xml A new multiplet table for FeI J/ApJS/94/221 J/ApJS/94/221 New multiplet table for FeI A new multiplet table for FeI G Nave S Johansson R C M Learner A P Thorne J W Brault Astrophys. J. Suppl. Ser. 94 221 1994 1994ApJS...94..221N Atomic physics atomic data line: identification We have recorded spectra of iron-neon and iron-argon hollow cathode lamps in the region 1700A-5um (59,000-2000cm^-1^), with Fourier transform (FT) spectrometers at the National Solar Observatory, Tucson, Arizona, and Imperial College, London, UK, and with a high-resolution grating spectrograph at the National Institute of Standards and Technology, Gaithersburg, Maryland. The uncertainty of the strongest lines in the FT spectra is less than 0.002cm^-1^ (0.2mA at 3000A; 8mA at 2um). Pressure- and current-dependent shifts are less than 0.001cm^-1^ for transitions between low-lying levels, increasing to 0.006cm^-1^ for transitions between the most highly excited levels. We report 28 new energy levels of Fe I and revised values of another 818 levels. We have identified 9501 lines as due to 9759 transitions in Fe I, and these are presented in the form of a new multiplet table and finding list. This compares with the ~5500 lines due to 467 energy levels in the multiplet tables of Moore (1950, NBS Circ., No.488 and 1959, NBS Tech. note 30). The biggest increase is in the near-ultraviolet and near infrared, and many of the new lines are present in the solar spectrum. Experimental log (gf) values are included where they are available. A further 125 unidentified lines due to Fe I are given.
Energy levels of FeI Config Assigned configuration --- Term Term, in order of lowest fine structure level --- J Level value --- n_J '*' for 28 unpublished energy levels --- Level Energy level cm-1 e_Level rms uncertainty on Level cm-1 New multiplet table for FeI Num Multiplet number --- Term1 First term designation --- n_Term1 Separation symbol '-' --- Term2 Second term designation --- J1 First J value --- n_J1 Separation symbol '-' --- J2 Second J value --- I Intensity of the line number=1 Intensity in arbitrary units. These are given as log(I) to two decimal places for FT spectra. Grating intensities are on a different scale to the FT intensities, and are from the continuous hollow cathode spectra, except those in parentheses, which are from the pulsed hollow cathode. Symbols are: d: diffuse; b: blended; *: unresolved; ?: questionable. --- Lvac Vacuum wavelength number=2 Vacuum wavelength is derived from the measured wavenumber, Sigma. Wavelengths measured in FT spectra are given to 4 decimal places and those measured in grating spectra to 3 decimal places in the UV. No grating spectra were recorded above 3250 A. 0.1nm Lair Air wavelength number=3 Air wavelengths for all lines above 2000 A have been derived from the wavenumbers using Edlen dispersion formula given as equation 2 in the printed paper. See also note (2). 0.1nm Lo-R Difference between observed and Ritz wavelengths number=4 Difference between observed wavelength and the Ritz wavelength derived from the energy levels in table 1. This difference should be subtracted from Lvac or Lair to obtain the Ritz wavelength. 0.1pm Sigma Measured wavenumber number=5 Wavenumbers measured in FT spectra are given to 3 decimal places and those measured in grating spectra to 2 decimal places. cm-1 q_Sigma Quality of Sigma number=6 Quality of measured wavenumber. A: Uncertainty < 0.005 cm-1. B: Uncertainty < 0.01 cm-1. C: Uncertainty < 0.02 cm-1. D: Uncertainty > 0.02 cm-1 or blended line Wavelength uncertainties are given in table 3. --- So-R Difference between observed and Ritz wavenumbers number=7 Difference between observed wavenumber and the Ritz wavenumber derived from the energy levels in table 1. This difference should be subtracted from Sigma to obtain the Ritz wavenumber. mK El Excitation potential of lower level of transition eV Eu Excitation potential of upper level of transition eV Elc El in units of cm-1 cm-1 Euc Eu in units of cm-1 cm-1 log(gf) Log of experimental gf values --- r_log(gf) Source of log(gf) value number=8 Sources for log(gf) values are: a: O'Brian et al., 1991, J. Opt. Soc. Am., B8, 1185 b: Fuhr et al., 1988, J. Phys. Chem. Ref. Data, 17, Suppl. 4 c: Meylan et al., 1993ApJS...85..163M d: Johansson et al., 1994ApJ...429..419J --- Blend Species of blended line number=9 Species of blended line: I: Line blended with another Fe I transition II: Line blended with Fe II transition Ne: Line blended with Ne line Ar: Line blended with Ar line R: Line is self-reversed. Ritz wavelengths and wavenumber are given. M: Line is masked by another line of the given species. --- Finding list Lambda Vacuum (<2000A) or air (>2000A) wavelength 0.1nm Sigma Wavenumber cm-1 Num Multiplet number --- Unidentified lines due to FeI I Intensity --- Lambda Air wavelength 0.1nm Sigma Wavenumber cm-1 Lee Brotzman ADS 10-Oct-94, Patricia Bauer CDS 1995 Feb 16 AAS CD-ROM series, Volume 3, 1995 J_ApJS_94_221.xml The Hawai K-band survey. III. Spectroscopy of K < 20 galaxies. J/ApJS/94/461 J/ApJS/94/461 The Hawai K-band survey. III. The Hawai K-band survey. III. Spectroscopy of K < 20 galaxies. A Songaila L L Cowie E M Hu J P Gardner Astrophys. J. Suppl. Ser. 94 461 1994 1994ApJS...94..461S Galaxies, photometry Photometry, infrared Redshifts Spectroscopy cosmology: observations galaxies: distances and redshifts galaxies: evolution infrared: galaxies surveys We present spectra and multicolor (B,I,K) data for near-infrared (K) selected spatially complete magnitude limited (K<20) galaxy samples from the Hawaii Survey. The redshift identification of the sample of 298 galaxies is substantially complete to a B magnitude of 26 and an I magnitude of 22.5, and identification of observed galaxies ranges from nearly 100% completeness at K<18 to ~70% completeness at K=19-20. We note that many of the unidentified objects appear to be red (I-K) objects which are flat in the optical and spectroscopically featureless. Strengths of spectral-line features and breaks are tabulated for the 262 galaxies with reasonably secure redshifts. The measured redshifts nearly all fall at z<1, with the exception of a compact absorption-line object at z=2.35. At K>=18, the redshift distribution is well fitted by a model with no luminosity evolution, implying that from the K-band Hubble diagram, the Hubble constant can vary at most by 10% over the redshift range from z~0.025 to 0.25, and that positive luminosity evolution at any significant level between z=0 and z=1 is ruled out. However, the evolution of both the emission-line strengths and the 4000{AA} break indicates that galaxies were undergoing significantly more star formation at z=1 than at the present time.
Redshift catalog for all fields sorted by K magnitude No Sequential number --- --- --- Note Original redshift number=1 Redshifts which are taken from the literature are marked by the object number according to the following code : LCG (Lilly, Cowie & Gardner, 1991ApJ...369...79L), CSH (Cowie, Songaila, & Hu, 1991Natur.354..460C), L (Lilly, 1993ApJ...411..501L), C (Cowie et al., 1994ApJ...434..114C). No spectra are given for these objects in Fig.3. --- Field Observed field number --- xpos Offset of the galaxy form the field center in x coordinate (East to the left) arcsec ypos Offset of the galaxy form the field center in y coordinate (North to the top) arcsec Kmag K magnitude mag Imag I magnitude mag Bmag B magnitude mag z Measured redshift --- u_z Uncertainty flag on z --- n_z n: object not identified --- Redshift distribution with K magnitude Kmin Minimum K magnitude for K interval mag Kmax Maximum K magnitude for K interval mag NTot Number of total galaxies --- NObs Number of spectroscopically observed galaxies --- NID Number of identified galaxies --- zmean Mean redshift of identified galaxies --- e_zmean rms uncertainty on zmean --- Zmed Median redshift of all observed galaxies --- zmedl Lower median redshift error bar --- zmedh Higher median redshift error bar --- Spectral features and breaks No Sequential number --- Kmag K magnitude mag z Redshift --- u_z Uncertainty flag on z --- n_z n: no id --- Break Strength of the 4000A break --- Mg Mgb index --- Na NaD line rest frame equivalent width 0.1nm GBand G band rest frame equivalent width 0.1nm Halpha H{alpha} + [N II] complex rest frame equivalent width 0.1nm Hbeta H{beta} line rest frame equivalent width 0.1nm [OII] [O II]{lambda}3727 rest frame equivalent width 0.1nm [OIII] [O III]{lambda}5007 rest frame equivalent width 0.1nm James Marcout, Patricia Bauer CDS 1997 Jul 11 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_94_461.xml A K' imaging survey of molecular outflow sources J/ApJS/94/615 J/ApJS/94/615 Molecular outflow sources A K' imaging survey of molecular outflow sources K -W Hodapp Astrophys. J. Suppl. Ser. 94 615 1994 1994ApJS...94..615H infrared: ISM: continuum ISM: jets and outflows ISM: molecules open clusters and associations: general stars: formation surveys The primary data for this paper consists of 232 FITS images containing the imaging data and frames of the standard stars. The standard star images are 60x60 pixels frames with the star approximately centered on the frame. The first seven characters of the standard star file names contain the name of the star, sometimes abbreviated. The last character of the file name (A, B, C, ...) distinguishes different frames of the same star. The exposure time (limited by the external shutter) is given in the file headers. The standard stars include GL 347A, HD 3029, HD 18881, HD 22686, HD 161903, HD 162208, HD 201941, HD 203856, and HD 225023. Object names, coordinates, file names and other pertinent information for the program objects are given in table 1 described below. A K'-band imaging survey with a ~8'x3' field of view of all regions associated with CO molecular outflow from the list of Fukui (1989) has been conducted. We present the individual images and describe individual nebulous objects and star clusters. The vast majority of all outflow sources are associated with nebulosity detectable in K', so such nebulae can be used as tracers for very young stars. We find a significant fraction (one-third) of molecular outflow sources to be associated with clusters of young stars. Most of the young embedded clusters show peaks in their K' magnitude histograms that, if interpreted as an evolutionary effect, indicate average ages of the embedded star population of <1x10^6yr.
List of objects Name Object name --- RAh Right Ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec File Filename (without .fit extension) --- Dist Distance kpc Neb Number of detected localized nebulae --- n_Neb Unknown value for DR21 --- Cluster 'cluster': outflow source associated with young cluster --- Peak Absolute magnitude of K' magnitude peak --- n_Peak 'n' if no absolute magnitude of K'mag peak --- afgl437.fit afgl437 data afgl490.fit afgl490 data afgl961.fit afgl961 data afgl2591.fit afgl2591 data afgl4029.fit afgl4029 data afgl5142.fit afgl5142 data afgl5157.fit afgl5157 data afgl5173.fit afgl5173 data afgl5180.fit afgl5180 data afgl6366.fit afgl6366 data as353.fit as353 data b5irs3.fit b5irs3 data b335.fit b335 data bd463471.fit bd463471 data bip14.fit bip14 data bnklori.fit bnklori data bsf56.fit bsf56 data cepa.fit cepa data cepc.fit cepc data cepe.fit cepe data cmawest.fit cmawest data dr21.fit dr21 data elias112.fit elias112 data g352074.fit g352074 data ggd4.fit ggd4 data ggd27.fit ggd27 data ggd1215.fit ggd1215 data gl347a_a.fit gl347a_a data gl347a_b.fit gl347a_b data gl347a_c.fit gl347a_c data gl347a_d.fit gl347a_d data gl347a_e.fit gl347a_e data gl347a_f.fit gl347a_f data gl347a_g.fit gl347a_g data gl347a_h.fit gl347a_h data gl347a_i.fit gl347a_i data gl347a_j.fit gl347a_j data gl347a_k.fit gl347a_k data gl347a_l.fit gl347a_l data gl347a_m.fit gl347a_m data gss30.fit gss30 data h161903a.fit h161903a data h161903b.fit h161903b data h161903c.fit h161903c data h161903d.fit h161903d data h161903e.fit h161903e data h161903f.fit h161903f data h161903g.fit h161903g data h161903h.fit h161903h data h162208a.fit h162208a data h162208b.fit h162208b data h162208c.fit h162208c data h162208d.fit h162208d data h162208e.fit h162208e data h201941a.fit h201941a data h201941b.fit h201941b data h203856a.fit h203856a data h203856b.fit h203856b data h203856c.fit h203856c data h203856d.fit h203856d data h203856e.fit h203856e data h225023a.fit h225023a data h225023b.fit h225023b data h225023c.fit h225023c data h225023d.fit h225023d data h225023e.fit h225023e data h225023f.fit h225023f data haro610.fit haro610 data haro4255.fit haro4255 data hd3029a.fit hd3029a data hd3029b.fit hd3029b data hd3029c.fit hd3029c data hd3029d.fit hd3029d data hd3029e.fit hd3029e data hd3029f.fit hd3029f data hd3029g.fit hd3029g data hd3029h.fit hd3029h data hd3029i.fit hd3029i data hd3029j.fit hd3029j data hd3029k.fit hd3029k data hd3029l.fit hd3029l data hd3029m.fit hd3029m data hd3029n.fit hd3029n data hd3029o.fit hd3029o data hd3029p.fit hd3029p data hd3029q.fit hd3029q data hd3029r.fit hd3029r data hd3029s.fit hd3029s data hd3029t.fit hd3029t data hd18881a.fit hd18881a data hd18881b.fit hd18881b data hd18881c.fit hd18881c data hd18881d.fit hd18881d data hd18881e.fit hd18881e data hd22686a.fit hd22686a data hd22686b.fit hd22686b data hd22686c.fit hd22686c data hd22686d.fit hd22686d data hd22686e.fit hd22686e data hd250550.fit hd250550 data hh12.fit hh12 data hh24.fit hh24 data hh26ir.fit hh26ir data hh711s13.fit hh711s13 data hlxztau.fit hlxztau data i00213.fit i00213 data i00259.fit i00259 data i01133.fit i01133 data i04191.fit i04191 data i20126.fit i20126 data i20188.fit i20188 data i23032.fit i23032 data i23139.fit i23139 data i23151.fit i23151 data ic1396e.fit ic1396e data ic1396n.fit ic1396n data ic1396w.fit ic1396w data ic1805w.fit ic1805w data ic2087.fit ic2087 data k350.fit k350 data l100.fit l100 data l146.fit l146 data l255.fit l255 data l379irs2.fit l379irs2 data l379irs3.fit l379irs3 data l483.fit l483 data l673.fit l673 data l723.fit l723 data l778.fit l778 data l810.fit l810 data l988a.fit l988a data l988e.fit l988e data l988f.fit l988f data l1036.fit l1036 data l1157.fit l1157 data l1172.fit l1172 data l1203.fit l1203 data l1204a.fit l1204a data l1204b.fit l1204b data l1206.fit l1206 data l1211.fit l1211 data l1221.fit l1221 data l1228.fit l1228 data l1251a.fit l1251a data l1251b.fit l1251b data l1262.fit l1262 data l1287.fit l1287 data l1293.fit l1293 data l1448c.fit l1448c data l1489.fit l1489 data l1535.fit l1535 data l1551ir5.fit l1551ir5 data l1594.fit l1594 data l1598.fit l1598 data l1598nw.fit l1598nw data l1617.fit l1617 data l1634.fit l1634 data l1641c.fit l1641c data l1641n.fit l1641n data l1641s.fit l1641s data l1641s2.fit l1641s2 data l1641s3.fit l1641s3 data l1641s4.fit l1641s4 data l1642.fit l1642 data l1654.fit l1654 data l1660.fit l1660 data l1709.fit l1709 data licha198.fit licha198 data licha234.fit licha234 data m8e.fit m8e data monob1d.fit monob1d data monob1g.fit monob1g data monob1h.fit monob1h data monob1i.fit monob1i data monr2.fit monr2 data monr2e.fit monr2e data morgan8.fit morgan8 data morgan9.fit morgan9 data morgan18.fit morgan18 data morgan54.fit morgan54 data morgan59.fit morgan59 data mwc1080.fit mwc1080 data ngc281e.fit ngc281e data ngc281w.fit ngc281w data ngc1333i.fit ngc1333i data ngc1999.fit ngc1999 data ngc2024.fit ngc2024 data ngc2068.fit ngc2068 data ngc2071.fit ngc2071 data ngc2071n.fit ngc2071n data ngc2264.fit ngc2264 data ngc6334.fit ngc6334 data ngc7129.fit ngc7129 data ngc7538.fit ngc7538 data omc2.fit omc2 data oriaeast.fit oriaeast data oriawest.fit oriawest data orii2.fit orii2 data pvcep.fit pvcep data rcra.fit rcra data rhooph1.fit rhooph1 data rhoophb.fit rhoophb data rhoophe.fit rhoophe data rhoophs.fit rhoophs data rmon.fit rmon data rno13.fit rno13 data rno15fir.fit rno15fir data rno43s.fit rno43s data rno73.fit rno73 data rno91.fit rno91 data s68.fit s68 data s87.fit s87 data s88b.fit s88b data s140.fit s140 data s140n.fit s140n data s187irs.fit s187irs data s233.fit s233 data s235b.fit s235b data s242.fit s242 data s287a.fit s287a data s287b.fit s287b data s287c.fit s287c data s287n.fit s287n data s254258.fit s254258 data serpsvs2.fit serpsvs2 data ttau.fit ttau data v645cyg.fit v645cyg data v1057cyg.fit v1057cyg data v1331cyg.fit v1331cyg data w3irs5.fit w3irs5 data w28a2.fit w28a2 data w49.fit w49 data w75n.fit w75n data zztau.fit zztau data Lee Brotzman ADS 29-Oct-94, Patricia Bauer CDS 1995 Feb 16 AAS CD-ROM series, Volume 3, 1995 Addresses: Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 J_ApJS_94_615.xml Old stellar populations. V. Absorption feature indices for the complete Lick/IDS sample of stars J/ApJS/94/687 J/ApJS/94/687 Old stellar populations. V. Old stellar populations. V. Absorption feature indices for the complete Lick/IDS sample of stars G Worthey S M Faber J J Gonzalez D Burstein Astrophys. J. Suppl. Ser. 94 687 1994 1994ApJS...94..687W galaxies: stellar content stars: abundances stars: fundamental parameters stars: general Detailed documentation has been supplied by the authors in file tablea1.doc. Twenty-one optical absorption features, 11 of which have been previously defined, are automatically measured in a sample of 460 stars. Following Gorgas et al., the indices are summarized in fitting functions that give index strengths as functions of stellar temperature, gravity, and [Fe/H]. This project was carried out with the purpose of predicting index strengths in the integrated light of stellar populations of different ages and metallicities, but the data should be valuable for stellar studies in the Galaxy as well. Several of the new indices appear to be promising indicators of metallicity for old stellar populations. A complete list of index data and atmospheric parameters is available in computer-readable form.
Collected indices for published stars HD Henry Draper Catalog number, if any --- Name1 Alternate names for the star number=1 Name1 and Name2 could be : "HR" numbers (Bright Star Catalog; Hoffleit 1982), "BD" (Bonner Durchmusterung) numbers, "Gl" numbers (Nearby Stars; Gleise 1969), cluster names (see the Appendix of the printed paper), or common names. This is not a complete cross-reference list. --- Name2 Alternate names for the star number=1 Name1 and Name2 could be : "HR" numbers (Bright Star Catalog; Hoffleit 1982), "BD" (Bonner Durchmusterung) numbers, "Gl" numbers (Nearby Stars; Gleise 1969), cluster names (see the Appendix of the printed paper), or common names. This is not a complete cross-reference list. --- CN1 CN1 index value mag CN2 CN2 index value mag Ca4227 Ca4227 index value 0.1nm G4300 G4300 index value 0.1nm Fe4383 Fe4383 index value 0.1nm Ca4455 Ca4455 index value 0.1nm Fe4531 Fe4531 index value 0.1nm Fe4668 Fe4668 index value 0.1nm HB4681 HB4681 index value 0.1nm Fe5015 Fe5015 index value 0.1nm Mg1 Mg1 index value mag Mg2 Mg2 index value mag Mgb Mgb index value 0.1nm Fe5270 Fe5270 index value 0.1nm Fe5335 Fe5335 index value 0.1nm Fe5406 Fe5406 index value 0.1nm Fe5709 Fe5709 index value 0.1nm Fe5782 Fe5782 index value 0.1nm Na5895 Na5895 index value 0.1nm TiO1 TiO1 index value mag TiO2 TiO2 index value mag Teff Effective temperature K logg Logarithm of the surface gravity cm/s2 [Fe/H] Metallicity --- Nobs Number of observations number=2 This number is the upper limit to the actual number of measurements which went into the index averages, as some portions of some spectra were missing or otherwise unusable. --- r_Teff Source for effective temperature number=3 See the author-supplied documentation, file tablea1.doc, for a complete list of references. There are 2 references in r_[Fe/H] for HD 114762 --- r_logg Source for gravity number=3 See the author-supplied documentation, file tablea1.doc, for a complete list of references. There are 2 references in r_[Fe/H] for HD 114762 --- r_[Fe/H] Source for [Fe/H] number=3 See the author-supplied documentation, file tablea1.doc, for a complete list of references. There are 2 references in r_[Fe/H] for HD 114762 --- Com Spectral type and comment, if any. --- tablea1.doc Author-supplied documentation Lee Brotzman ADS 16-Oct-94, Francois Ochsenbein CDS 1995 Jul 24 AAS CD-ROM series, Volume 3, 1995 J_ApJS_94_687.xml The luminosity function at the end of the main sequence: results of a deep, large-area, CCD survey for cool dwarfs. J/ApJS/94/749 J/ApJS/94/749 RI photometry of cool dwarfs The luminosity function at the end of the main sequence: results of a deep, large-area, CCD survey for cool dwarfs. J D Kirkpatrick J T McGraw T R Hess J Liebert D W McCarthy Jr. Astrophys. J. Suppl. Ser. 94 749 1994 1994ApJS...94..749K I/98 : NLTT Catalogue (Luyten, 1979) J/AJ/106/773 : Mass-luminosity relation (Henry+, 1993) Photometry, RI Stars, dwarfs Stars, late-type stars: low-mass, brown dwarfs stars: luminosity function, mass function The luminosity function at the end of the main sequence is determined from V, R, and I data taken by the CCD/Transit Instrument (CTI), a dedicated telescope surveying an 8.25' wide strip of sky centered at {delta}=+28deg, thus sampling Galactic latitudes of +90deg down to -35deg. A selection of 133 objects chosen via R-I and V-I colors has been observed spectroscopically at the 4.5m Multiple Mirror Telescope to assess contributions by giants and subdwarfs and to verify that the reddest targets are objects of extremely late spectral class. Eighteen dwarfs of type M6 or later have been discovered, with the latest being of type M8.5. Data used for the determination of the luminosity function cover 27.3deg^2^ down to a completeness limit of R=19.0. This luminosity function, computed a V, I, and bolometric magnitudes, shows an increase at the lowest luminosities, corresponding to spectral types later than M6, an effect suggested in earlier work by Reid & Gilmore and Leggett & Hawkins. When the luminosity function is segregated into north Galactic and south Galactic portions, it is found that the upturn at faint magnitudes exists only in the southern sample. In fact, no dwarfs with M_I_>=12.0 are found within the limiting volume of the 19.4deg^2^ northern sample, in stark contrast to the smaller 7.9deg^2^ area at southerly latitudes where seven such dwarfs are found. This fact, combined with the fact that the Sun is located ~10-40pc north of the midplane, suggests that the latest dwarfs are part of a young population with a scale height much smaller than the 350pc value generally adopted for other M dwarfs. These objects comprise a young population either because the lower metallicities prevalent at earlier epochs inhibited the formation of late M dwarfs or because the older counterparts of this population have cooled beyond current detection limits. The latter scenario would hold if these late-type M dwarfs are substellar. The luminosity function data together with an empirical derivation of the mass-luminosity relation (from Henry & McCarthy, 1993, Cat. <J/AJ/106/773>) are used to compute a mass function independent of theory. This mass function increases toward the end of the main sequence, but the observed density of M dwarfs is still insufficient to account for the missing mass. If the increases seen in the luminosity and mass functions are indicative of a large, unseen, substellar population, brown dwarfs may yet add significantly to the mass of the Galaxy.
Stars from the NLTT catalog (Cat. <I/98>) that should be in the CTI strip Object Object name --- mr Red magnitude number=1 Magnitudes as listed in the NLTT catalogue (Cat. <I/98>). mag mpg Photographic magnitude number=1 Magnitudes as listed in the NLTT catalogue (Cat. <I/98>). mag col Luyten's color class --- pm Total proper motion arcsec/yr RAh Right ascension (1987.5) number=2 Predicted coordinates for epoch and equinox 1987.5. h RAm Right ascension (1987.5) number=2 Predicted coordinates for epoch and equinox 1987.5. min RAs Right ascension (1987.5) number=2 Predicted coordinates for epoch and equinox 1987.5. s DEd Declination (1987.5) number=2 Predicted coordinates for epoch and equinox 1987.5. deg DEm Declination (1987.5) number=2 Predicted coordinates for epoch and equinox 1987.5. arcmin DEs Declination (1987.5) number=2 Predicted coordinates for epoch and equinox 1987.5. arcsec CTI CTI name --- n_CTI Note number=3 c: In Table 1. d: Luyten 1979 (Cat. <I/98>) appears to have overestimated this object's proper motion. The CTI star listed in the table has been confirmed from CTI images to be the proper motion object (LP 323-25 = LHS 2723) in question. --- l_Rmag Limit flag on Rmag --- Rmag CTI R (or V if n_Rmag=V) magnitude mag n_Rmag V: CTI V magnitude in Rmag column --- R-I CTI R-I colour index mag e_R-I rms uncertainty on R-I mag Note Notes --- James Marcout, Patricia Bauer CDS 1997 Jun 24 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_94_749.xml An atlas of ultraviolet P Cygni profiles J/ApJS/95/163 J/ApJS/95/163 Ultraviolet P Cygni profiles An atlas of ultraviolet P Cygni profiles T P Snow H J G L M Lamers D M Lindholm A P Odell Astrophys. J. Suppl. Ser. 95 163 1994 1994ApJS...95..163S Spectra, ultraviolet Stars, early-type atlases line: profiles stars: early-type ultraviolet: stars In addition to the tabular data described below, spectra for the 232 stars in this atlas are included from Figure 2 of the printed paper, as well as the 16 H-R diagrams from Figure 3. The spectra are contained in Postscript files named 'star_nnn.ps', where 'nnn' represents a number from '001' to '232', inclusive. The H-R diagrams are contained in Postscript files named 'hrnnnn.ps', where 'nnnn' represents a number corresponding to the wavelength of the ion in question, e.g. 'hr1640.ps' is the H-R diagram for He II at 1640 Angstroms. The H-R diagram for all atlas stars (Figure 1 in the printed paper) is given in file 'hrall.ps'. We have selected spectra of 232 stars from the IUE archives for inclusion in an atlas intended for various uses but tailored especially for the study of stellar winds. The atlas covers the range in spectral types from O3 to F8. The full atlas covers the reduced and normalized high resolution spectra from the IUE long- and short-wavelength spectrographs. Here we discuss the selection of the stars and the data reduction, and we present in velocity units the profiles of lines formed in the stellar winds. The selected lines cover a wide range of ionizations, allowing a comparison of the profiles from different ions in the wind of each star and a comparison of the different wind lines as a function of spectral type and luminosity. We also present the basic data on the program stars to facilitate study of the dependence of wind features on stellar parameters such as luminosity, temperature, escape velocity, and v sin i. We provide an overview of the characteristic behavior of the wind lines in the H-R diagram. The complete spectra are available in digital form through the NASA Astrophysics Data System (ADS). We offer a description of the electronic database that is available through the ADS and guidelines for obtaining access to that database.
Atlas stars and IUE observations Num Star number --- HR Bright Star Catalog <V/50> number --- HD Henry Draper Catalog <III/135> number --- m_HD HD Catalog component --- Name Star name --- Sp Spectral type --- IUE IUE image number --- Ap Aperture --- Date Exposure date, DD-MMM-YYYY "DD-MMM-YYYY" Time Exposure time, HH:MM:SS "HH:MM:SS" Texp Length of exposure s FileName Spectrum filename in subdirectory sp --- Basic properties of atlas stars Num Star number --- HD Henry Draper Catalog number --- m_HD HD Catalog component --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec Sp Spectral type --- V V magnitude mag B-V B-V color mag E(B-V) E(B-V) value --- MV Absolute visual magnitude mag m-M Distance modulus mag n_m-M Note on cluster member number=1 'c' indicates a cluster member from the catalog of Humphreys, R.M. (1978ApJS...38..309H) --- Teff Effective temperature K BC Bolometric correction mag Mbol Bolometric magnitude mag Mstar Stellar mass solMass Rstar Stellar radius Sun Gamma Gravity reduction due to radiation pressure --- Vesc Escape velocity km/s RV Radial velocity km/s Bin Indication of binarity number=2 For B, A, and F stars, information about binarity is from the Bright Star Catalog. For most O stars (those with V<8), this information was obtained from Gies, D.R. (1987ApJS...64..545G) --- l_vsini Limit flag for v sin i --- vsini v sin i km/s u_vsini Uncertainty flag for v sin i --- Lines selected for this atlas Ion Ion for selected line --- Lambda Wavelength of selected line 0.1nm Remark Remark on selected line --- EP Excitation potential, lower level of transition eV gt Statistical weight, lower level of transition --- f Oscillator strength of the line --- Sp Spectral types plotted --- table2.tex LaTeX version of Table 2 table3.tex LaTeX version of Table 3 table4.tex LaTeX version of Table 4 hr1175.ps Lambda 117.5nm HR diagram hr1206.ps Lambda 120.6nm HR diagram hr1240.ps Lambda 124.0nm HR diagram hr1335.ps Lambda 133.5nm HR diagram hr1338.ps Lambda 133.8nm HR diagram hr1371.ps Lambda 137.1nm HR diagram hr1400.ps Lambda 140.0nm HR diagram hr1530.ps Lambda 153.0nm HR diagram hr1550.ps Lambda 155.0nm HR diagram hr1640.ps Lambda 164.0nm HR diagram hr1670.ps Lambda 167.0nm HR diagram hr1718.ps Lambda 171.8nm HR diagram hr1858.ps Lambda 185.8nm HR diagram hr2586.ps Lambda 258.6nm HR diagram hr2800.ps Lambda 280.0nm HR diagram hrall.ps All HR diagrams Lee Brotzman ADS 16-Nov-94, Francois Ochsenbein CDS 1996 Sep 03 Addresses: Snow T.P. <tsnow@casa.colorado.edu Lindholm D.M. <lind@ncar.ucar.edu> Center for Astrophysics and Space Astronomy, Campus Box 389, University of Colorado, Boulder, CO 80309. Lamers H.J.G.L.M. <hennyl@sron.ruu.nl Astronomical Institute and SRON Laboratory for Space Research, University of Utrecht, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands Odell A.P. <odell@nauvax.ucc.nau.edu> Department of Physics and Astronomy, Northern Arizona University, P.O. Box 6010, Flagstaff, AZ 86011-6010. UNKNOWN UNKNOWN * 16-Nov-1994: Lee Brotzman, for AAS CD-ROM series, Volume 3, 1995. * 03-Sep-1996: The "Num" value in table2.dat, and the (RA DE) position in table3,dat were added at CDS. J_ApJS_95_163.xml Atlas of Quasar Energy Distributions J/ApJS/95/1 J/ApJS/95/1 Atlas of Quasar Energy Distributions Atlas of Quasar Energy Distributions M Elvis B J Wilkes J C McDowell R F Green J Bechtold S P Willner M S Oey E Polomski R Cutri Astrophys. J. Suppl. Ser. 95 1 1994 1994ApJS...95....1E Infrared sources QSOs Radio sources Ultraviolet X-ray sources atlases galaxies: photometry quasars: general We present an atlas of the spectral energy distributions (SEDs) of normal, non-blazar, quasars over the whole available range (radio to 10 keV X-rays) of the electromagnetic spectrum. The primary (UVSX) sample includes 47 quasars for which the spectral energy distributions include X-ray spectral indices and UV data. Of these, 29 are radio quiet, and 18 are radio loud. The SEDs are presented both in figures and in tabular form, with additional tabular material published on CD-ROM. Previously unpublished observational data for a second set of quasars excluded from the primary sample are also tabulated. The effects of host galaxy starlight contamination and foreground extinction on the UVSX sample are considered and the sample is used to investigate the range of SED properties. Of course, the properties we derive are influenced strongly by the selection effects induced by quasar discovery techniques. We derive the mean energy distribution (MED) for radio-loud and radio-quiet objects and present the bolometric corrections derived from it. We note, however, that the dispersion about this mean is large (~one decade for both the infrared and ultraviolet components when the MED is normalized at the near-infrared inflection). At least part of the dispersion in the ultraviolet may be due to time variability, but this is unlikely to be important in the infrared. The existence of such a large dispersion indicates that the MED reflects only some of the properties of quasars and so should be used only with caution.
Adopted X-ray power-law fits Name Quasar name --- l_F0.2 Limit flag for F2 flux --- F0.2 Flux at 0.2 KeV uJy E_F0.2 Error in F2 flux (upper limit) uJy e_F0.2 Error in F2 flux (lower limit) uJy alpha10 Energy index at 1 keV --- E_alpha10 Error in energy index alpha10 (upper limit) --- e_alpha10 Error in energy index alpha10 (lower limit) --- F10 Flux at 1 keV or lower limit of the flux if interval uJy n_F10 Separation when interval of flux at 1 keV --- F10u Upper limit of the flux when interval uJy E_F10 Error in F10 flux (upper limit) uJy e_F10 Error in F10 flux (lower limit) uJy Ref Reference number=1 1) This paper; 2) Wilkes and Elvis (1987ApJ...323..243W) 3) Masnou et al. (1992A&A...253...35M) 4) Elvis et al. (1991ApJ...378..537E) 5) Comastri et al. (1992ApJ...384...62C) 6) Turner and Pounds (1989MNRAS.240..833T) 7) Williams et al. (1992ApJ...389..157W) 8) Ohashi et al. (1992ApJ...398...87O) 9) Della Ceca et al., Cat. <VII/181> 10) Turner and Pounds (1988MNRAS.232..463T) 11) Tananbaum et al. (1986ApJ...305...57T) 12) Saxton et al. (1993MNRAS.262...63S) --- alpha40 Energy index at 40 keV --- E_alpha40 Error in energy index alpha40 (upper limit) --- e_alpha40 Error in energy index alpha40 (lower limit) --- l_F40 Limit flag on F40 flux --- F40 Flux at 4 keV or lower limit of the flux if interval uJy n_F40 Separation when interval of flux at 4 keV --- F40u Upper limit of the flux F40 when interval uJy e_F40 rms uncertainty on F40 flux uJy ref2 Reference for F40 flux --- Observational details for new X-ray power-law fits Name Quasar name --- Seq Sequence number --- Date Observation date --- Exp Exposure time s Gain Gain --- PHA PHA channels --- Counts Fit counts --- Rate Count rate ct/s alpha Spectral index --- NH Hydrogen column density 10+20cm-2 ki2 Ki2 number=1 See Wilkes & Elvis (1987ApJ...323..243W) for details --- Adopted continuum bands Lambda Nominal Wavelength number= Continuum spectrophotometry has been binned into the rest frame bandpass defined by this table, chosen to avoid strong emission lines as described in the text. Avoiding: 1000-1050 L-beta 1150-1275 L-alpha 1215/NV (20000 km/s) 1375-1450 OIV 1402 1500-1600 CIV 1550 1850-1950 CIII 1909 2700-2900 Mg II 2798 3300-3550 NeV 3426 3650-3750 [OIII] 3727 3850-4450 Ne II 3869, 3968, H delta 4101, H gamma 4340 4650-5100 H Beta 4861 OIII 6250-6850 OI 6300, Halpha 6562 0.1nm Range1 Wavelength range (lower value) number= Continuum spectrophotometry has been binned into the rest frame bandpass defined by this table, chosen to avoid strong emission lines as described in the text. Avoiding: 1000-1050 L-beta 1150-1275 L-alpha 1215/NV (20000 km/s) 1375-1450 OIV 1402 1500-1600 CIV 1550 1850-1950 CIII 1909 2700-2900 Mg II 2798 3300-3550 NeV 3426 3650-3750 [OIII] 3727 3850-4450 Ne II 3869, 3968, H delta 4101, H gamma 4340 4650-5100 H Beta 4861 OIII 6250-6850 OI 6300, Halpha 6562 0.1nm --- Separation flag number= Continuum spectrophotometry has been binned into the rest frame bandpass defined by this table, chosen to avoid strong emission lines as described in the text. Avoiding: 1000-1050 L-beta 1150-1275 L-alpha 1215/NV (20000 km/s) 1375-1450 OIV 1402 1500-1600 CIV 1550 1850-1950 CIII 1909 2700-2900 Mg II 2798 3300-3550 NeV 3426 3650-3750 [OIII] 3727 3850-4450 Ne II 3869, 3968, H delta 4101, H gamma 4340 4650-5100 H Beta 4861 OIII 6250-6850 OI 6300, Halpha 6562 --- Range2 Wavelength range (upper value) number= Continuum spectrophotometry has been binned into the rest frame bandpass defined by this table, chosen to avoid strong emission lines as described in the text. Avoiding: 1000-1050 L-beta 1150-1275 L-alpha 1215/NV (20000 km/s) 1375-1450 OIV 1402 1500-1600 CIV 1550 1850-1950 CIII 1909 2700-2900 Mg II 2798 3300-3550 NeV 3426 3650-3750 [OIII] 3727 3850-4450 Ne II 3869, 3968, H delta 4101, H gamma 4340 4650-5100 H Beta 4861 OIII 6250-6850 OI 6300, Halpha 6562 0.1nm IUE continuum bands Name QSO name --- Obs Observation date "MM/YY" Exp1 First exposure --- Exp2 Second exposure --- Lambda Lambda (rest) 0.1nm log(nu) Observed frequency Hz log(nuFnu) Flux in the observed frame Jy.Hz e_log(nuFnu) rms uncertainty on log(nuFnu) Jy.Hz Optical continuum measurements Name QSO name --- Date Observation date --- Exp Exposure --- Lambda Lambda (rest) nm log(nu) Observed frequency Hz log(nuFnu) Flux in the observed frame Jy.Hz e_log(nuFnu) rms uncertainty on log(nuFnu) Jy.Hz Adopted extinction law Ref Extinction law reference number=1 RL85: Rieke and Lebofsky 1985 SM79: Savage and Mathis 1979 --- log(nu) Frequency Hz R(nu) Extinction relative to extinction at V (A(nu)/A(V)) --- Starlight Template log(nu) Frequency Hz log(nuLnu) Energy distribution of starlight template used for host galaxy subtraction, normalized at V Hz.solLum Observed energy distribution Name Quasar name --- log(nu0) Frequency nu0 Hz log(nu1) Frequency nu1 Hz log(nu2) Frequency nu2 Hz l_log(nuFnu) Limit flag on log(nuFnu) --- log(nuFnu) Flux Jy.Hz E_log(nuFnu) Error on lognuFnu (upper limit) Jy.Hz e_log(nuFnu) Error on lognuFnu (lower limit) Jy.Hz Date Observation date "DD/MM/YY" Aper Aperture arcsec Filt Filter or detector --- Inst Intrument or telescope --- Ref References --- Near-infrared photometry Name Quasar name --- Jmag J (1.24um) magnitude mag u_Jmag Uncertainty flag on J magnitude --- e_Jmag rms uncertainty on J magnitude mag Hmag H (1.63um) magnitude mag u_Hmag Uncertainty flag on H magnitude --- e_Hmag rms uncertainty on H magnitude mag Kmag K (2.19um) magnitude mag u_Kmag Uncertainty flag on K magnitude --- e_Kmag rms uncertainty on K magnitude mag l_3.4mag limit flag on 3.4um magnitude --- 3.4mag 3.4um magnitude (Delta{lambda}=0.2um) mag u_3.4mag Uncertainty flag on 3.4um magnitude --- e_3.4mag rms uncertainty on 3.4mag or error upper limit if e(3.4mag)l not blank mag e(3.4mag)l Error in 3.4mag (lower limit) mag L'mag L' (3.79um) magnitude mag e_L'mag rms uncertainty on L' magnitude mag Date Observation date --- Tel Telescope --- Beam Beam size arcsec Note When a, a 5" aperture was used for the 3.4um band measurement. When c: possible clouds, uncertainties believed adequate --- Radio fluxes Name Quasar name --- l_Nu Limit flag on nu --- Nu Frequency GHz l_Score Limit flag on Score --- Score Core flux number=1 The division of fluxes into core and extended is arbitrary when only low-resolution observations are available. In such case the presence of a flux in the 'core' column indicates we have chosen to use it in the construction of the energy distribution. mJy e_Score rms uncertainty on Score mJy l_Sext Limit flag on Sext --- Sext Extended flux number=1 The division of fluxes into core and extended is arbitrary when only low-resolution observations are available. In such case the presence of a flux in the 'core' column indicates we have chosen to use it in the construction of the energy distribution. mJy e_Sext rms uncertainty on Sext mJy Date Observation date number=2 MM/YY for a month of observation YY for a year of observation YY-YY for several years of observation "MM/YY" u_Date Uncertainty flag on year of observation --- Tel Telescope number=3 Telescope acronyms are: FCRAO: Five College Radio Astronomy Observatory, MA GB: Green Bank 300 foot telescope NRAO: NRAO Green Bank Interferometer, WVA OVRO: Owens Valley Radio Observatory, CA PKS: Parkes 64-m DSN telescope, NSW, Australia VLA: Very Large Array, NM VLBI: Goldstone and Madrid DSN telescopes WSRT: Westerbork Synthesis Radio Telescope, Netherlands. --- l_Res Limite flag on resolution --- Res Resolution arcsec u_Res Uncertainty flag on resolution --- Ref References number=4 1: Kellerman et al. (1989AJ.....98.1195K) 2: I. Gioia, private communication 3: Gower and Hutchings (1984AJ.....89.1658G) 4: Unger et al. (1987MNRAS.228..521U) 5: Preston et al. (1985AJ.....90.1599) 6: Feigelson, Isobe and Kembhavi (1984AJ.....89.1464F) 7: Rudnick, Sitko, and Stein (1984AJ.....89..753R) 8: Miley and Hartsuijker (1978A+AS...34..129M) 9: Price and Milne (1965AuJPh..18..329P) 10: Pooley and Henbest (1974MNRAS.169..477P) 11: Perley (1982AJ.....87..859P) 12: Spencer et al. (1989MNRAS.240..657S) 13: Swarup, Sinha, and Hilldrup (1984MNRAS.208..813S) 14: Wills (1979ApJS...39..291W) 15: Owen, Porcas and Neff (1978AJ.....83.1009O) 16: Hintzen, Ulvestad and Owen (1983AJ.....88..709H) 17: Antonucci and Barvainis (1988ApJ...325L..21A) 18: Hutchings and Gower (1985AJ.....90..405H) 19: Shimmins and Bolton (1981AuJPh..34..471S) 20: Bolton and Butler (1975AuJPA..34...33B) 21: Wills (1975AuJPS..38....1W) 22: Ekers (1969AuJPS...7....1E) 23: Shimmins and Bolton (1972AuJPS..23....1S) 24: Shimmins and Bolton (1972AuJPS..26....1S) 25: Meurs and Wilson (1981A+AS...45...99M) 26: Edelson (1987ApJ...313..651E) 27: Gregory and Condon (1991) Cat. <VIII/14> 28: White and Becker Cat. <J/MNRAS/251/330> 29: Wright et al. Cat. <J/MNRAS/251/330> 30: Jagers et al. (1982A+A...105..279J) 31: Bolton et al. (1971AuJPh..24..889B) 32: Shimmins et al. (1966AuJPh..19..837S) 33: Barvainis and Antonucci (1989ApJS...70..257B) --- Millimeter fluxes Name Quasar name --- lambda Line mm l_S Limit flag on flux --- S Flux at lambda mJy e_S rms uncertainty on flux mJy Date Obsercation date yr Tel Telescope --- Ref References number=1 1) Antonucci, Barvainis and Alloin (1990) (1990ApJ...353..416A) 2) Barvainis and Antonucci (1989) (1989ApJS...70..257B) 3) Chini, Kreysa and Biermann (1989) (1989A&A...219...87C) 4) Clegg, et al. (1983) (1983ApJ...273...58C) 5) Edelson, Malkan and Rieke (1987) (1987ApJ...321..233E) 6) Engargiola et al. (1988) (1988ApJ...332L..19E) 7) Ennis, Neguebauer and Werner (1982) (1982ApJ...262..460E) 8) Landau, Epstein and Rather (1980) 9) Owen, et al. (1978) 10) Owen and Puschell (1982) 11) Robson, et al. (1985) (1985MNRAS.213..355R) 12) Steppe, et al. (1988) (1988A&AS...75..317S) --- Magnitude scale zero points Band Band --- Lambda Reference lambda um Zeropt1 Zero point (Vega) number=1 The zero points correspond to a system in which the magnitude of Vega is exactly zero. Values are given for an object with the same spectrum as Vega and for an object with a flat energy distribution (power-law spectrum F_{nu}_~{nu}^-{alpha}^ of slope unity) Jy Zeropt2 Zero point (alpha = 1) number=1 The zero points correspond to a system in which the magnitude of Vega is exactly zero. Values are given for an object with the same spectrum as Vega and for an object with a flat energy distribution (power-law spectrum F_{nu}_~{nu}^-{alpha}^ of slope unity) Jy Adopted host galaxy parameters Name Object name --- logL H band luminosity number=1 Adopted luminosities and half light radii for host galaxies, derived as discussed in the text. solLum E_logL Error in logL (upper limit) solLum e_logL Error in logL (lower limit) solLum Rad Half-light radius number=1 Adopted luminosities and half light radii for host galaxies, derived as discussed in the text. kpc Ref References number=2 No spatial information was available for objects marked with reference (0), and they have been assigned the median luminosity of the remainder of the sample. 1: Boroson, Oke and Green (1982) (1982ApJ...263...32B) 2: Gehren et al. (1984) (1984ApJ...278...11G) 3: Smith et al. (1986) (1986ApJ...306...64S) 4: Boroson and Oke (1984) (1984ApJ...281..535B) 5: McAlary et al. (1983) (1983ApJS...52..341M) 6: Neugebauer et al. (1985) (1985ApJ...298..275N) 7: Yee and Green (1987) (1987AJ.....94..618Y) 8: Hutchings, Crampton and Campbell (1984) (1984ApJ...280...41H) 9: Griersmith and Visvanathan (1979) (1979A&A....79..329G) --- table3.tex LaTeX version of table3 table6.tex LaTeX version of table6 table9.tex LaTeX version of table9 table10.tex LaTeX version of table10 table11.tex LaTeX version of table11 table12.tex LaTeX version of table12 CDS 1996 Feb 22 AAS CD-ROM series, Volume 3, 1995 Lee Brotzman [ADS] 13-Nov-94 J_ApJS_95_1.xml The Second Caltech-Jodrell Bank VLBI Survey. I. Observations of 91 of 193 Sources J/ApJS/95/345 J/ApJS/95/345 Second Caltech-Jodrell Bank VLBI Survey. I. The Second Caltech-Jodrell Bank VLBI Survey. I. Observations of 91 of 193 Sources G B Taylor R C Vermeulen T J Pearson A C S Readhead D R Henstock I W A Browne P N Wilkinson Astrophys. J. Suppl. Ser. 95 345 1994 1994ApJS...95..345T J/ApJS/98/1 : First Caltech-Jodrell Bank VLBI Survey. I. (Polatidis+ 1995) J/ApJS/98/33 : First Caltech-Jodrell Bank VLBI Survey. II. (Thakkar+ 1995) J/ApJS/99/297 : First Caltech-Jodrell Bank VLBI Survey. III (Xu+ 1995) J/ApJS/100/1 : Second Caltech-Jodrell Bank VLBI Survey. II. (Henstock+ 1995) QSOs Radio sources VLBI galaxies: structure quasars: general radio continuum: galaxies surveys techniques: interferometric We define the sample for the second Caltech-Jodrell Bank VLBI survey. This is a sample of 193 flat- or gigahertz-peaked-spectrum sources selected at 4850 MHz. This paper presents images of 91 sources with a resolution of ~1 mas, obtained using VLBI observations at 4992 MHz with a global array. The remaining images and the integrated radio spectra will be presented in a forthcoming paper by Henstock et al.
The CJ2 sample Source B1950 source name according to IAU convention number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- RAh Right ascension, J2000 The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> h RAm Right ascension, J2000 number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> min RAs Right ascension, J2000 number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> s DE- Declination sign, always blank number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- DEd Declination, J2000 number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> deg DEm Declination, J2000 number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> arcmin DEs Declination, J2000 number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> arcsec S80cm Total flux density at 80 cm number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- S20cm Total flux density at 20 cm Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- S6cm Total flux density at 6 cm Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- S3.6cm Total flux density at 3.6 cm number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- IDopt Optical identification Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- Rmag Apparent R magnitude number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> mag n_z Indicates a featureless spectrum number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- z Redshift Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- Date Date of VLBI observations number= The position for one source 0256+424 was off in Patnaik et al. (1992MNRAS.254..655P) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. Noteono S80cm: Total flux density at 80cm from J. Douglas, private communication. number= Total flux density at 20cm from White & Becker (1992) Cat. <VIII/17> number= Total flux density at 6cm from Gregory & Condon (1991) Cat. <VIII/14> Noteono S3.6cm: Total flux density at 3.6cm from Kuhr et al. (1981AJ.....86..854K) or JVAS (Patnaik et al. 1992MNRAS.254..655P) number= Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar G - Galaxy BL - BL Lac object EF - Empty Field BS - Blue stellar object BO - Blue object RS - Red stellar object RO - Red object NS - Neutral stellar object NO - Neutral object Noteono Rmag: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. number= Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 Cat. <VII/166> --- Telescope characteristics Tel Telescope name --- Code Code used number=1 B = Max-Planck-Institut fur Radioastronomie O = Onsaa Space Observatory W = Westerbork Synthesis Radio Telescoper, NFRA J2, C = Nuffield Radio Astronomy Laboratories L, N = Instituto di Radioastronomia G = National Radio Astronomy Observatory K = Haystack Observatory BR,FD,HN,KP,LA,NL,OV,PT,SC = National Radio Astronomy Observatory VLBA Y = National Radio Astronomy Observatory VLA --- Loc Location of each telescope --- Diam Diameter of each telescope m n_Diam x when two values --- Diam2 Diameter when two values m Jun1992 Session Jun 1992 success number=2 " indicates whether the telescope participated successfully in that session. --- Sep1992 Session Sep 1992 success number=2 " indicates whether the telescope participated successfully in that session. --- Mar1993 Session Mar 1993 success number=2 " indicates whether the telescope participated successfully in that session. --- TsysK System temperature in K number=3 The values quoted are representative of the three sessions. The VLA was used in single-antenna mode. K TsysJy System temperature in Jy number=3 The values quoted are representative of the three sessions. The VLA was used in single-antenna mode. Jy Sens Sensitivity of the system K/Jy *Map parameters Source B1950 source name according to IAU convention number= Data are in mJy/beam --- Date Date of VLBI observation number= Data are in mJy/beam --- Dur Duration on source of VLBI observation number= Data are in mJy/beam min a FWHM of major axis of the restoring beam number= Data are in mJy/beam mas b FWHM of minor axis of the restoring beam number= Data are in mJy/beam mas PA Position angle of major axis, north through east number= Data are in mJy/beam deg S4.85GHzn Peak flux density, naturally weighted map Data are in mJy/beam number= Data are in mJy/beam mJy e_S4.85GHzn Off source rms, naturally weighted map number= Data are in mJy/beam mJy S4.85GHznC First contour, percent of peak flux density number= Data are in mJy/beam % S4.85GHzt Peak flux density, tapered map number= Data are in mJy/beam mJy e_S4.85GHzt Off source rms, tapered map number= Data are in mJy/beam mJy S4.85GHztC First contour, % of peak flux density number= Data are in mJy/beam % Gaussian models CJ2 B1950 source name according to IAU convention number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. --- S Flux density of component number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. Jy Rad Radius of component Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. mas Theta Angle to component number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. deg a FWHM of major axis of component number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. mas b/a Axial ratio of major to minor axis, b/a number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. --- Phi Position angle of major axis, North through East number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. deg Amp Amplitude agreement factor number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. --- Phase Closure phase agreement factor number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. --- Total Total agreement factor number= Radius of component, measured from position of first component. Noteono Theta: Angle to component, measured North through East from the position of the first component. --- James Marcout, Patricia Bauer CDS 1996 Oct 24 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 07-May-95 UNKNOWN UNKNOWN * 29-Apr-1997: table2 added at CDS (J. Marcout, CDS) J_ApJS_95_345.xml Position angles and alignments of clusters of galaxies J/ApJS/95/401 J/ApJS/95/401 Clusters of galaxies position angles Position angles and alignments of clusters of galaxies M Plionis Astrophys. J. Suppl. Ser. 95 401 1994 1994ApJS...95..401P Clusters, galaxy galaxies: clusters: general galaxies: fundamental parameters The position angles of a large number of Abell and Shectman clusters, identified in the Lick map as surface galaxy-density enhancements, are estimated. I determine the major axis orientation of a total of 637 clusters, of which 448 are Shectman clusters (202 of which are also Abell clusters) and 189 are Abell clusters not originally detected by Shectman due to his adopted density threshold. Using published redshifts for 277 of these clusters I have detected strong nearest neighbor alignments over scales up to ~15h^-1^Mpc at a>~2.5-3{sigma} significance level, while quite weak alignments are detected even up to ~60h^-1^Mpc. A more significant alignment signal (~4{sigma}) is detected among all neighbors residing in superclusters and having separations <~ 10h^-1^Mpc. Again, weaker but significant alignments are found when larger separations are considered. Since my cluster sample is neither volume limited nor redshift complete (which would have tended to wash out any real alignment signal), the alignments detected should reflect a real and possibly a stronger underline effect.
Mean position angles of Abell and Shectman clusters identified at the 3.6 level Shect Cluster Shectman number (1985ApJS...57...77S) --- Abell Cluster Abell number (Cat. <VII/4>) --- Level Number of levels number=1 Number of overdensity levels used to estimate the position angle --- Ncells Number of cells, minimum if n_Ncells='-' number=2 Minimum and maximum number of 10'x10' cells, Ncells, defining the cluster sampling area (at the different overdensity levels). --- --- - for interval --- Ncells2 Maximun number of cells --- PA Position angle deg e_PA rms uncertainty on PA number=3 For the cases were the position angle was determined in three or more overdensity levels, the error and the median value are also listed. In those cases where four levels were used, we average the two central PA values deg PAMed Median position angle number=3 For the cases were the position angle was determined in three or more overdensity levels, the error and the median value are also listed. In those cases where four levels were used, we average the two central PA values deg Position angles of Abell clusters, identified at the 3.6 level but estimated at the 2.5 level Position angles of Abell clusters, identified at the 3.6 level but estimated at the 1.8 level *Position angles of Abell clusters, identified at the 2.5 level but estimated at the 1.8 level Abell Abell number --- Ncells Number of cells --- PA Position angle deg Patricia Bauer CDS 1997 May 30 UNKNOWN UNKNOWN Prepared via OCR at CDS. * 20-Jul-1998: several OCR errors corrected thanks to the catalog A222 supplied by A. Andernach originated from Manolis Plionis <plionis@sapfo.astro.noa.gr> J_ApJS_95_401.xml Molecular clouds in Cygnus. I. A large-scale ^13^CO survey. J/ApJS/95/419 J/ApJS/95/419 Molecular clouds in Cygnus. I. Molecular clouds in Cygnus. I. A large-scale ^13^CO survey. K Dobashi J -P Bernard Y Yonekura Y Fukui Astrophys. J. Suppl. Ser. 95 419 1994 1994ApJS...95..419D Carbon monoxide Interstellar medium Radio sources catalogs ISM: clouds ISM: molecules A large-scale 13CO(J=1-0) survey was performed with a 2.7' angular resolution toward the Cygnus region, using the two 4-m millimeter telescopes at Nagoya University. An area of 432deg^2^ was covered with an 8' grid spacing, and 24,300 positions were observed. Significant 13CO emission (>1.2K.km/s=3{sigma}) is detected at 2191 positions, corresponding to a detection rate of 9%. On the basis of the ^13^CO data, 159 distinct clouds are identified. Physical properties of these clouds such as molecular column densities, sizes, and masses are derived for the individual clouds. Astronomical objects associated with the molecular clouds were searched for in the literature. Seven H II regions, three SNRs, 45 T Tauri-type stars, 18 molecular outflows, and 215 IRAS point sources selected as candidates for protostars are likely to be associated with the molecular clouds. This paper presents the observational technique used for this survey and a complete list of the detected molecular clouds in Cygnus.
A catalog of ^13^CO clouds Seq Sequential number --- Note Note number=1 a: There is a secondary velocity component at V_LSR_=-2.8 km/s at the peak position of Cloud 8 (081.9+00.8). Clouds 8 and 34 comprise more than one velocity components (see text). --- Name Cloud name --- RAh Peak right ascension of the ^13^CO cloud (1950) h RAn Peak right ascension of the ^13^CO cloud (1950) min RAs Peak right ascension of the ^13^CO cloud (1950) s DEd Peak declination of the ^13^CO cloud (1950) deg DEm Peak declination of the ^13^CO cloud (1950) arcmin DEs Peak declination of the ^13^CO cloud (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Tr* Temperature K DV {DELTA}V km/s Vlsr V_lsr_ km/s I Intensity K.km/s tau(CO) ^13^CO optical depth --- N(CO) ^13^CO column density 10+15cm-2 N(H2) H_2_ column density 10+21cm-2 l_size Limit flag on size --- size Size number=2 Size of the ^13^CO clouds measured at 1.2K.km/s contours in Fig. 1 (3{sigma}). arcmin --- multiplication sign --- size2 Size number=2 Size of the ^13^CO clouds measured at 1.2K.km/s contours in Fig. 1 (3{sigma}). arcmin Dist Distance kpc l_Mass Limit flag on Mass --- Mass Cloud mass solMass ref References number=3 References to the adopted distances: 1: Dame & Thaddeus (1985ApJ...297..751D) 2: Blitz et al. (1982ApJS...49..183B) 3: Lada (1985ARA&A..23..267L) 4: Fischer et al. (1985ApJ...293..508F) 5: Bally & Scoville (1980ApJ...239..121B) 6: Tatematsu et al. (1990A&A...237..189T) 7: Yun & Clemens (1992ApJ...385L..21Y) 8: Clark (1986A&A...164L..19C) 9: Walker (1959ApJ...130...57W) 10: Dobashi et al. (1992AJ....104.1525D) 11: Elias (1978ApJ...223..859) 12: Fukui et al. (1993, in Protostras and planets III, ed. E. Levy, Tuscon: Arizona Univ. Press, 603 13: Humphreys (1978ApJS...38..309H) 14: Sugitani et al. (1991ApJS...77...59S) 15: Sugitani et al. (1989ApJ...342L..87S) 16: Lindblad et al. (1973A&A....24..309L) -- Associated astronomical objects Seq Sequential number --- Cloud Cloud name --- RAh Peak right ascension of the ^13^CO cloud (1950) h RAn Peak right ascension of the ^13^CO cloud (1950) min RAs Peak right ascension of the ^13^CO cloud (1950) s DEd Peak declination of the ^13^CO cloud (1950) deg DEm Peak declination of the ^13^CO cloud (1950) arcmin DEs Peak declination of the ^13^CO cloud (1950) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg HII Associated HII region in Sharpless (1959, Cat. <VII/20>) --- SNRs Associated supernova remnant in Green (1988Ap&SS.148....3G) --- Rim The clouds having counterparts among bright rimmed globules are denoted by "yes" --- HBC T Tauri stars catalogued in Herbig & Bell (1988, Cat. <V/73>) associated with the cloud --- IPS Number of associated IRAS point sources (Cat. <II/125>) --- n_IPS ns: cloud out of the coverage of the IRAS PSC (Cat. <II/125>) --- Outflows Associated molecular outflows found in the surveyed region. --- Lynds Associated darks clouds in Lynds (1962, cat. <VII/7>) --- James Marcout, Patricia Bauer CDS 1997 May 22 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_95_419.xml IRAS images of nearby dark clouds J/ApJS/95/457 J/ApJS/95/457 IRAS images of nearby dark clouds IRAS images of nearby dark clouds D O S Wood P C Myers D A Daugherty Astrophys. J. Suppl. Ser. 95 457 1994 1994ApJS...95..457W II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) Infrared sources Interstellar medium dust, extinction infrared: ISM: continuum ISM: molecules We have investigated ~100 nearby molecular clouds using the extensive, all-sky database of IRAS. The clouds in this study cover a wide range of physical properties including visual extinction, size, mass, degree of isolation, homogeneity and morphology. IRAS 100 and 60 micrometre co-added images were used to calculate the 100 micrometre optical depth of dust in the clouds. These images of dust optical depth compare very well with ^12^CO and ^13^CO observations, and can be related to H_2_ column density. From the optical depth images we locate the edges of dark clouds and the dense cores inside them. We have identified a total of 43 "IRAS clouds" (regions with Av>2) which contain a total of 255 "IRAS cores" (regions with Av>4) and we catalog their physical properties. We find that the clouds are remarkably filamentary, and that the cores within the clouds are often distributed along the filaments. The largest cores are usually connected to other large cores by filaments. We have developed selection criteria to search the IRAS Point Source Catalog for stars that are likely to be associated with the clouds and we catalog the IRAS sources in each cloud or core. Optically visible stars associated with the clouds have been identified from the Herbig and Bell catalog. From these data we characterize the physical properties of the clouds including their star-formation efficiency.
IRAS
Field studied Name Field name --- RAh Center right ascension (1950) h RAm Center right ascension (1950) min DE- Center declination sign --- DEd Center declination (1950) deg DEm Center declination (1950) arcmin GLON Galactic longitude deg GLAT Galactic latitude deg Dim1 Dimension deg --- --- Dim2 Dimension deg *Flat-fielding and background subtraction Field Field name --- oRA1 Point 1 R.A. offset number=1 Blank: no flat field subtraction arcmin oDE1 Point 1 D.E. offset number=1 Blank: no flat field subtraction arcmin S100um1 Point 1 100{mu}m flux number=1 Blank: no flat field subtraction MJy/sr S60um1 Point 1 60{mu}m flux number=1 Blank: no flat field subtraction MJy/sr oRA2 Point 2 R.A. offset number=1 Blank: no flat field subtraction arcmin oDE2 Point 2 D.E. offset number=1 Blank: no flat field subtraction arcmin S100um2 Point 2 100{mu}m flux number=1 Blank: no flat field subtraction MJy/sr S60um2 Point 2 60{mu}m flux number=1 Blank: no flat field subtraction MJy/sr oRA3 Point 3 R.A. offset number=1 Blank: no flat field subtraction arcmin oDE3 Point 3 D.E. offset number=1 Blank: no flat field subtraction arcmin S100um3 Point 3 100{mu}m flux number=1 Blank: no flat field subtraction MJy/sr S60um3 Point 3 60{mu}m flux number=1 Blank: no flat field subtraction MJy/sr oRAB Background subtraction R.A. offset arcmin oDEB Background subtraction D.E. offset arcmin S100umB Background subtraction 100{mu}m flux MJy/sr S60umB Background subtraction 60{mu}m flux MJy/sr IRAS clouds (Av > 2 mag) Cloud Cloud name number=1 Name of the constellation where the cloud is located followed by a single letter where A is the most massive cloud we identified in that constellation, B is the second most massive and so on. --- Dist Assumed distance to the cloud pc RAhB Bottom left field right ascension (1950) h RAmB Bottom left field right ascension (1950) min RAsB Bottom left field right ascension (1950) s DE-B Bottom left field declination sign --- DEdB Bottom left field declination (1950) deg DEmB Bottom left field declination (1950) arcmin DEsB Bottom left field declination (1950) arcsec RAhT Top right field right ascension (1950) h RAmT Top right field right ascension (1950) min RAsT Top right field right ascension (1950) s DE-T Top right field declination sign --- DEdT Top right field declination (1950) deg DEmT Top right field declination (1950) arcmin DEsT Top right field declination (1950) arcsec Area Total area of the cloud pc+2 Tau100 Mean 100{mu}m optical depth 10-6 l_Mass Limit flag on Mass --- Mass H_2_ total mass solMass Note Notes number=2 1: The cloud is truncated by one or more image edges. 2: Part or all of the cloud lies in the region of overlap between two images. 3: Cloud mass is an upper limit due to significant heating by embedded stars. --- IRAS cores (Av > 4 mag) Core Core name number=1 Name of the core which is the name of the parent cloud (table4) followed by a number, 1 is the most massive core in the cloud, 2 is the next most massive core and so on. --- RAhP Peak 100um optical depth right ascension (1950) h RAmP Peak 100um optical depth right ascension (1950) min RAsP Peak 100um optical depth right ascension (1950) s DE-P Peak 100um optical depth declination sign --- DEdP Peak 100um optical depth declination (1950) deg DEmP Peak 100um optical depth declination (1950) arcmin DEsP Peak 100um optical depth declination (1950) arcsec TauMax Maximal optical depth in the core (in {mu}neper) 10-6 T(TauMax) Dust temperature at the position of TauMax K RAhE Ellipse right ascension (1950) number=2 Parameters of an ellipse that fit to each core by eye. h RAmE Ellipse right ascension (1950) number=2 Parameters of an ellipse that fit to each core by eye. min RAsE Ellipse right ascension (1950) number=2 Parameters of an ellipse that fit to each core by eye. s DE-E Ellipse declination sign number=2 Parameters of an ellipse that fit to each core by eye. --- DEdE Ellipse declination (1950) number=2 Parameters of an ellipse that fit to each core by eye. deg DEmE Ellipse declination (1950) number=2 Parameters of an ellipse that fit to each core by eye. arcmin DEsE Ellipse declination (1950) number=2 Parameters of an ellipse that fit to each core by eye. arcsec MajAxis Ellipse major axis number=2 Parameters of an ellipse that fit to each core by eye. pc MinAxis Ellipse minor axis number=2 Parameters of an ellipse that fit to each core by eye. pc PA Ellipse position angle (deg E of N) number=2 Parameters of an ellipse that fit to each core by eye. deg Area Core area pc+2 l_MassC Limit flag on MassC --- MassC Total mass of the core solMass N Mean core column density 10+21cm-2 HD Number of associated stars from HD catalogue --- IRAS Numer of IRAS PSC associations --- l_Mass Limit flag on Mass --- Mass Total mass of all IRAS stars associated with the core solMass l_Lum Limit flag on Lum --- Lum Total luminosity of all IRAS stars associated with the core solLum Note Notes number=3 1: The cloud is truncated by one or more image edges. 2: Part or all of the cloud lies in the region of overlap between two images. 3: Core mass is an upper limit due to significant heating by embedded stars --- James Marcout, Patricia Bauer CDS 1997 Mar 25 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_95_457.xml Infrared CO line list for the X ^1^{Sigma}^+^ state J/ApJS/95/535 J/ApJS/95/535 Infrared CO line list for X 1{Sigma}+ state Infrared CO line list for the X ^1^{Sigma}^+^ state D Goorvitch Astrophys. J. Suppl. Ser. 95 535 1994 1994ApJS...95..535G Atomic physics Radio lines molecular data A complete line list with improved accuracy for all the rotation- vibration transitions of the fundamental, first, and second overtone bands up to nu=20 and J=149 of the ground state X ^1^{Sigma}^+^ of the seven CO isotopes - 12C16O, 13C16O, 12C17O, 12C18O, 13C18O, 14C16O, and 13C17O - is made available to the astronomical community. A line list of the pure rotational transitions up to nu=5 and J=60 is also made available for these seven isotopes. This line list contains the transition frequency, the lower state energy, the Einstein A-value, the gf-value, the transition strength at 3000K or 1000K for the pure rotational transitions, the expectation value of the effective dipole moment operator, and the quantum numbers of each transition. Individual partition functions are reported in the temperature range of 500 to 10,000K.
Transition frequencies, gf values, and J values for the bandheads of the R-branch overtone bands of 12C16O v Lower state vibrational quantum number --- sigma1 Frequency, fundamental cm-1 log(gf1) gf-value, fundamental --- J1 J-value, fundamental --- sigma2 Frequency, first overtone cm-1 log(gf2) gf-value, first overtone --- J2 J-value, first overtone --- sigma3 Frequency, second overtone cm-1 log(gf3) gf-value, second overtone --- J3 J-value, second overtone --- Rotationless dipole moments, M(0), for the pure rotational transitions (D) v Vibrational quantum number --- M26 Rotationless dipole moment, 12C16O D M36 Rotationless dipole moment, 13C16O D M28 Rotationless dipole moment, 12C18O D M27 Rotationless dipole moment, 12C17O D M38 Rotationless dipole moment, 13C18O D M46 Rotationless dipole moment, 14C16O D M37 Rotationless dipole moment, 13C17O D Polynomial fits to [F(m)]^{1/2} for the pure rotational transitions Isotope Code for the isotope, e.g. '26' for 12C16O --- v Vibrational quantum number --- b0 b_0 coefficient --- b1 b_1 coefficient --- b2 b_2 coefficient --- b3 b_3 coefficient --- b4 b_4 coefficient --- Line list of 12C16O Delta v = +1 transitions Line list of 12C16O Delta v = +2 transitions Line list of 12C16O Delta v = +3 transitions sigma Transition frequency cm-1 R2 Expectation value, effective electric dipole matrix operator squared D2 A Einstein transition probability (A-value) Hz E Lower state term energy, lowest level = 0 cm-1 log(gf) gf-value --- S Strength evaluated at T = 3000 K cm/mol vu Upper state vibrational quantum number --- vl Lower state vibrational quantum number --- Type Transition type --- Jl Lower state angular momentum number --- </tableLink> <tableLink xlink:href="table2.dat"> <title/> </tableLink> <tableLink xlink:href="table3.dat"> <title/> </tableLink> <tableLink xlink:href="table4.dat"> <title/> </tableLink> <tableLink xlink:href="table5.dat"> <title/> </tableLink> </tableLinks> <fields> <field> <name>sigma</name> <definition>Transition frequency</definition> <units>cm-1</units> </field> <field> <name>R2</name> <definition>Expectation value, effective electric dipole matrix operator squared</definition> <units>D2</units> </field> <field> <name>A</name> <definition>Einstein transition probability (A-value)</definition> <units>Hz</units> </field> <field> <name>E</name> <definition>Lower state term energy, lowest level = 0</definition> <units>cm-1</units> </field> <field> <name>log(gf)</name> <definition>gf-value</definition> <units>---</units> </field> <field> <name>S</name> <definition>Strength evaluated at T = 3000 K</definition> <units>cm/mol</units> </field> <field> <name>vu</name> <definition>Upper state vibrational quantum number</definition> <units>---</units> </field> <field> <name>vl</name> <definition>Lower state vibrational quantum number</definition> <units>---</units> </field> <field> <name>Type</name> <definition>Transition type</definition> <units>---</units> </field> <field> <name>Jl</name> <definition>Lower state angular momentum number</definition> <units>---</units> </field> <field> <name>Isotope</name> <definition>Code for the isotope, e.g. '26' for 12C16O</definition> <units>---</units> </field> </fields> </tableHead> <textFile xlink:href="readme.doc"> <name>readme.doc</name> <description> <para>Author-supplied documentation</para> </description> </textFile> <textFile xlink:href="table6.tex"> <name>table6.tex</name> <description> <para>LaTeX version of Table 6</para> </description> </textFile> <textFile xlink:href="table7.tex"> <name>table7.tex</name> <description> <para>LaTeX version of Table 7</para> </description> </textFile> <textFile xlink:href="table8.tex"> <name>table8.tex</name> <description> <para>LaTeX version of Table 8</para> </description> </textFile> <textFile xlink:href="table9.tex"> <name>table9.tex</name> <description> <para>LaTeX version of Table 9</para> </description> </textFile> <textFile xlink:href="table10.tex"> <name>table10.tex</name> <description> <para>LateX version of Table 10</para> </description> </textFile> <textFile xlink:href="table11.tex"> <name>table11.tex</name> <description> <para>LaTeX version of Table 11</para> </description> </textFile> <history> <ingest> <creator> <lastName>Lee Brotzman</lastName> <affiliation>ADS</affiliation> </creator> <creator> <lastName>16-Nov-94, Patricia Bauer</lastName> <affiliation>CDS</affiliation> </creator> <date> <year>1995</year> <month>Feb</month> <day>16</day> </date> <acknowledgement>AAS CD-ROM series, Volume 3, 1995 Author's Address: Goorvitch D. <goorvitch@cma.arc.nasa.gov> Space Sciences Division, NASA Ames Research Center, Moffett Field, CA 94035-1000</acknowledgement> </ingest> </history> <identifier>J_ApJS_95_535.xml</identifier> </dataset> <dataset subject="astronomy" xmlns:xlink="http://www.w3.org/XML/XLink/0.9"> <title>K-Band Galaxy Counts J/ApJS/96/117 J/ApJS/96/117 K-Band Galaxy Counts K-Band Galaxy Counts B A McLeod G M Bernstein M J Rieke E V Tollestrup G G Fazio Astrophys. J. Suppl. Ser. 96 117 1995 1995ApJS...96..117M Galaxies, IR galaxies: general infrared: galaxies We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.
*MMT catalog ID Identification --- RAh Right ascension (2000) h RAm R.A. min RAs R.A. s DE- Declination sign, always blank --- DEd Declination (2000) deg DEm Dec. arcmin DEs Dec. arcsec Kmag K magnitude mag e_Kmag K error mag Her 1 catalog ID Identification number --- Class Class code Class code (based on colors) are: g = Galaxy; s = Star; t = star saturated on Bj, R, and I CCD frames, colors are incorrect --- RAh Right ascension (2000) h RAm R.A. min RAs R.A. s DE- Declination sign, always blank --- DEd Declination (2000) deg DEm Dec. arcmin DEs Dec. arcsec Kmag K magnitude mag e_Kmag K error mag I-K I-K color mag e_I-K I-K error mag R-I R-I color mag e_R-I R-I error mag Bj-I Bj-I color mag e_Bj-I Bj-I error mag SA57SO catalog ID Identification number --- Class Class code, g = Galaxy; s = Star --- RAh Right ascension (2000) h RAm R.A. min RAs R.A. s DE- Declination sign, always blank --- DEd Declination (2000) deg DEm Dec. arcmin DEs Dec. arcsec Kmag K magnitude mag e_Kmag K error mag J-K J-K color mag e_J-K J-K error mag Bj-K Bj-K color mag e_Bj-K Bj-K error mag CDS 1996 Jun 18 UNKNOWN UNKNOWN * 07-May-1995: Preparation by Lee Brotzman [ADS], AAS CD-ROM series, Volume 4, 1995 * 18-Jun-1996: Correction in table3.dat: MMTL-20 appeared twice in the original table3; its second occurrence was changed into MMTL-30. J_ApJS_96_117.xml Recalibration of the H_-0.5_-magnitudes of spiral galaxies J/ApJS/96/123 J/ApJS/96/123 H-magnitudes of spiral galaxies Recalibration of the H_-0.5_-magnitudes of spiral galaxies G Tormen D Burstein Astrophys. J. Suppl. Ser. 96 123 1995 1995ApJS...96..123T VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991) VII/75 : Infrared Photometry & 21cm data for nearby galaxies (Aaronson+, 1982) Aaronson (A99) 1977Thesi.........A Aaronson et al., (A1) 1979ApJ...229....1A Aaronson et al., (A2) 1980ApJ...237..655A Mould et al. (A3) 1980ApJ...238..458M Aaronson et al., (A4) 1980ApJ...239...12A Aaronson et al., (A5) 1981MNRAS.195p...1A Aaronson et al., (A6) 1982ApJ...258...64A Aaronson et al., (A7) 1982ApJS...50..241A, Cat. <VII/75> Aaronson et al., (A8) 1983ApJ...265....1A Aaronson (A9) 1986, in Galaxy Distances and Deviations from Universal Expansion, Ed. B.F. Madore & R.B. Tully (Dosdrecht: Reidel), 55 Aaronson et al., (A10) 1986ApJ...302..536A Aaronson et al., (A11) 1986ApJ...303....1A Cornell et al., (A12) 1987ApJS...64..507C Aaronson et al., (A13) 1989ApJ...338..654A Bothun et al., (A14) 1984ApJ...278..475B Bothun & Gould, (A15) 1987ApJ...313..629B Bothun et al., (A16) 1985ApJS...57..423B Galaxies, IR Galaxies, photometry Radial velocities galaxies: photometry infrared: galaxies The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. <VII/155>), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, & Corwin 1976, Cat .<VII/112>), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5<=log(A/D_g_)<=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.
H-Band aperture measurements Name Galaxy name --- S Source of observation number=1 1: Aaronson et al., 1979ApJ...229....1A 2: Aaronson et al., 1980ApJ...237..655A 3: Mould et al., 1980ApJ...238..458M 4: Aaronson et al., 1980ApJ...239...12A 5: Aaronson et al., 1981MNRAS.195p...1A 6: Aaronson et al., 1982ApJ...258...64A 7: Aaronson et al., 1982ApJS...50..241A, Cat. <VII/75> 8: Aaronson et al., 1983ApJ...265....1A 9: Aaronson 1986, in Galaxy Distances and Deviations from Universal Expansion, Ed. B.F. Madore & R.B. Tully (Dosdrecht: Reidel), 55 10: Aaronson et al., 1986ApJ...302..536A 11: Aaronson et al., 1986ApJ...303....1A 12: Cornell et al., 1987ApJS...64..507C 13: Aaronson et al., 1989ApJ...338..654A 14: Bothun et al., 1984ApJ...278..475B 15: Bothun & Gould, 1987ApJ...313..629B 16: Bothun et al., 1985ApJS...57..423B 99: Aaronson, 1977, Ph.D. Thesis, Harvard Univ. --- T Photometric numerical type --- n_T *: no value --- Hmag H magnitude measuring within aperture A mag e_Hmag rms uncertainty on Hmag mag log[A/D] Aperture size to fiducial optical diameter ratio --- n_log[A/D] *: no value --- magdif Difference between individual aperture measurement minus fitted growth curve mag n_magdif *: no value --- Derived and catalog parameters for H-Band observed galaxies Name Galaxy name --- PGC PGC (Cat. <VII/119>) number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec C Code for cluster or group assignement number=1 The numerical coding of cluster and group names is as follows: -1: Not classified 0: Not assigned 1: Pisces 2: A400 3: A539 4: Cancer 5: A1367 6: Coma 7: Z74-23 8: Hercules 9: Pegasus 10: A2634/66 12: Hydra 13: N3557 14: Cen 30 15: Cen 45 16: Antlia 17: ESO 508 18: Pavo 51: Local calibrators 52: Virgo, main cluster 53: N1023 54: Eridanus 55: Fornax 56: Leo 57: Ursa major 58: Coma I 59: Virgo, south 60: N5566 Group 61: Grus 62: N24/45 63: N134 64: N701/755 65: N2336 66: N2841 67: N3079/U5459 68: N3184 69: N3521 70: Leo Triplet 71: Can Van I 72: N5033 73: M51 74: N5371 75: N5364 76: N5676 77: N5866 78: N6070 79: N7370/7331 80: N7537/7541 --- TypeRC3 RC3 (Cat. <VII/155>) type --- T Photometric type --- n_T * when photometric type changed from that given by Hubble type --- Ext Blue magnitude Galactic extinction --- log(Dg) Fuducial corrected isophotal diameter [0.1arcmin] n_log(Dg) *: Diameter from Aaronson et al. else from RC3 (Cat. <VII/155>) or ESO catalogues --- logR Axial ratio R_25_=log(a/b) --- n_logR *: axial ratio from Aaronson et al. else from RC3 (Cat. <VII/155>) --- i Inclination deg HRV Heliocentric radial velocity km/s dVr Raw H I velocity width, not corrected for inclination km/s log(dV) Inclination-corrected HI velocity width, using inclination i, and corrected for heliocentric redshift [km/s] Hg Fiducial H-magnitude, corrected only for Galactic extinction, H^g^_0.5_ mag n_Hg *: optical data derived from Aaronson et al. --- Q Quality paramater for H^g^_0.5_ --- N Number of H-magnitude observations that defined the growth curve from which H^g^_0.5_ was derived --- U Code for inclusion or exclusion of a galaxy in the final IRTF sample number=2 G: included in the final IRTF sample F: too face-on N: no HI velocity width in Aaronson et al. papers P: Hubble type of P, I0 or L --- iA Inclination form Aaronson et al. survey deg log(dV)A H I velocity width corrected for the inclination, form Aaronson et al. survey [km/s] logD1 Fudicial corrected optical diameter defined by Aaronson et al. [0.1arcmin] H0 Corrected H magnitude used by Aaronson et al., H^0^_0.5_ --- James Marcout, Patricia Bauer CDS 1997 Sep 29 UNKNOWN UNKNOWN Prepared via OCR at CDS. In table4, for Z476112, misprint in position, 233845 +256130 instead of 233845 +251630 J_ApJS_96_123.xml Kinematics of Metal-Poor Stars in the Galaxy J/ApJS/96/175 J/ApJS/96/175 Kinematics of Metal-Poor Stars Kinematics of Metal-Poor Stars in the Galaxy T C Beers J Sommer-Larsen Astrophys. J. Suppl. Ser. 96 175 1995 1995ApJS...96..175B stars: kinematics stars: Population II We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] <= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 <= [Fe/H] <= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage & Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] <= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 <= [Fe/H] <= -0.6 and |z| <= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] <= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 <= [Fe/H] <= -1.5 and [Fe/H] <= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r > 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.
Positions, radial velocities, distances, and abundances Star Star name --- RAh Right ascension (1950.0) h RAm R.A. min RAs R.A. s DE- Declination sign --- DEd Declination (1950.0) deg DEm Dec. arcmin Vmag V magnitude mag Type Object classification Object classification codes: A = Apparent main-sequence A-type star AGB = asymptotic giant branch star D = main-sequence dwarf star FHB = field horizontal-branch star G = giant star SG = subgiant star TO = main-sequence turnoff star V = RR Lyraes and other variable stars --- RV Best available heliocentric radial velocity km/s Dist Distance from Sun pc [Fe/H] Abundance estimate Sun r_RV Source code for RV Source codes are listed in Table 1 of Beers and Sommer-Larsen (1995). --- r_Dist Source code for Dist --- r_[Fe/H] Source code for Fe/H --- UNKNOWN 1995 Jul 12 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 08-May-95 J_ApJS_96_175.xml Calibrating the broad band X-ray telescope. J/ApJS/96/303 J/ApJS/96/303 Calibrating Broad Band X-ray Telescope Calibrating the broad band X-ray telescope. K A Weaver K A Arnaud E A Boldt D Christian M Corcoran S S Holt K Jahoda R Kelley F E Marshall R F Mushotzky R Petre G Rawley P J Serlemitsos E M Schlegel A P Smale J H Swank A E Szymkowiak Astrophys. J. Suppl. Ser. 96 303 1995 1995ApJS...96..303W X-ray sources instrumentation: detectors space vehicles X-rays: general This paper describes the calibration of the two solid-state Si(Li) X-ray detectors and the X-ray telescopes that flew as part of Goddard Space Flight Center's Broad Band X-Ray Telescope (BBXRT) experiment on board the space shuttle Columbia in 1990 December. During the 9 day shuttle mission, BBXRT performed ~150 observations of 82 celestial sources. The content of the archive is summarised here. Although BBXRT had a relatively short life, it stands as a milestone in X-ray astronomy as being the first instrument to offer moderate spectral resolution over a wide bandpass (0.3-12.0keV). Among other things, this paper discusses the effective area calibration of the instrument, the flux calibration and flux corrections for off-axis observations, the detector background, and optimal background subtraction techniques. The on-axis effective area calibration for the central detector elements was performed using data from the Crab Nebula, while other carefully selected targets were used for calibration of the outer detector elements. The remaining systematic uncertainties in the effective area calibration for point sources observed both on and off axis are generally less than 5%-10%. The energy scale is known to better than 0.5% at 6.0 keV for both detectors. The results presented here have an impact on the calibration of other medium resolution X-ray experiments such as the CCDs on board ASCA (Astro-D) as well as the Advanced X-Ray Astrophysics Facility detectors.
Broad Band X-Ray Telescope (BBXRT) observation Log Source Source name --- RAdeg Nominal right ascension (1950.0) deg DEdeg Nominal declination (1950.0) deg DRA Offset in right ascension number=1 Offset of the pointing direction of the A-system telescope from the nominal RA and DE (epoch 1950.0), given as RAnom - RAaspect, and DEnom - DEaspect. Numbers are supplied only if there exists an aspect solution derived from data taken with the aspect camera. Specific details about aspect solutions can be obtained through the HEASARC at GSFC. deg DDE Offset in declination number=1 Offset of the pointing direction of the A-system telescope from the nominal RA and DE (epoch 1950.0), given as RAnom - RAaspect, and DEnom - DEaspect. Numbers are supplied only if there exists an aspect solution derived from data taken with the aspect camera. Specific details about aspect solutions can be obtained through the HEASARC at GSFC. deg Roll Roll angle of the A-system telescope (phi) number=2 If no aspect solution exists, the roll angle is only an approximate value. deg Start Start time of MET measured from 1990 December 2, 06:49:01 UT d ExpTime Exposure time s D/N Indicator of shuttle day or night number=3 N = night D = day MN = mostly night (>75%) MD = mostly day (>75%) B = both, mixed --- GR Mean detector guard rate number=4 Parameter that measures the rate of particle interactions with the guard. --- Angle Average off-axis angle number=5 Average off-axis angle (THETA) as derived rom the nominal and aspect RA.s and DE.s (cols. [2]-[5]). When an angle but no RA or DE offset is given, that angle is derived from ray tracing. A value of -1 indicates that the angle has not yet been calculated. A ray-tracing program is available from the HEASARC that allows observers to determine their own off-axis angles and to confirm our aspect solutions. arcmin Rate Total count rate in all 10 pixels. ct/s Class Type of object. --- James Marcout, Patricia Bauer CDS 1997 Aug 28 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_96_303.xml The Catalog of Southern Ringed Galaxies J/ApJS/96/39 J/ApJS/96/39 The Catalog of Southern Ringed Galaxies. The Catalog of Southern Ringed Galaxies R Buta Astrophys. J. Suppl. 96 39 1995 1995ApJS...96...39B Galaxies, ring Galaxy catalogs The Catalog of Southern Ringed Galaxies (CSRG) is a comprehensive compilation of diameters, axis ratios, relative bar position angles, and morphologies of inner and outer rings, pseudorings, and lenses in 3,692 galaxies south of declination -17 degrees. The catalog is based on visual inspection of most of the 606 fields of the SRC-J southern sky survey, with the ESO-B, ESO-R, and Palomar Sky surveys used as auxiliaries when needed for overexposed core regions. The catalog is most complete for SRC fields 1--303 (mostly south of declination -42 degrees). There are two auxiliary tables: Table 4 includes the notes for 371 entries in the main catalog, and Table 6 includes classifications for 859 additional galaxies not part of the main catalog. Detailed analysis of 5403 duplicate estimates of ring diameters and 1606 duplicate estimates of bar/ring position angles indicates that the CSRG has very good internal precision and homogeneity in these parameters. For an ``average'' ring or lens of angular diameter 0.'6 and apparent axis ratio 0.8, the internal errors are 0.'026 in angular diameter and 6.3 degrees in bar/ring position angle. Based on a comparison with two other major sources of ring diameter measurements, the external mean error in CSRG diameters is ~3.2 times the internal error at a given diameter. Comparison of the type classifications with other catalogues indicates good agreement on interpretations of features, including family and variety.
Catalog of Southern Ringed Galaxies RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Name Object Name --- O Outer feature classification R1, R1', R2', and R1R2' are OLR subclasses (Buta and Crocker 1991, AJ, 102, 1715) For 78 galaxies classified as having R1R2' features, data for the R2' part is continued after column 16 in the exact same format; the data for the R1 part are in bytes 46-64; the R1R2' classification is split across the record L refers to outer lens RL- refers to RL with R underlined; RL+ refers to RL with L underlined RG refers to ring galaxy PR refers to polar ring --- Family Family classification SX- means SAB with A underlined; SX means SAB with no underlines; and SX+ means SAB with B underlined --- I Inner feature classification rs- means rs with r underlined and rs+ means rs with s underlined l refers to inner lens rl- means rl with r underlined and rl+ means rl with l underlined rpl means pseudoring-lens --- T Numerical stage index Numerical stage index on scale of Third Reference Catalogue of Bright Galaxies (de Vaucouleurs et al. 1991, Springer: New York) --- u_T Uncertainty on T index --- D(O) Outer feature major axis diameter arcmin u_D(O) Uncertainty on D(O) --- d(O) Outer feature minor axis diameter arcmin u_d(O) Uncertainty on d(O) --- Thet(O) Relative bar/outer feature major axis position angle deg u_Thet(O) Uncertainty on Thet(O) --- Peculiar Peculiar or disturbed-looking --- D(I) Inner feature major axis diameter arcmin u_D(I) Uncertainly on D(I) --- d(I) Inner feature minor axis diameter arcmin u_d(I) Uncertainty on d(I) --- Thet(I) Relative bar/inner feature major axis position angle deg u_Thet(I) Uncertainty on Thet(I) --- Mult Multiplicity of spiral pattern Number of spiral arms n+ means n or more arms f means flocculent (see Elmegreen and Elmegreen, 1982, MNRAS, 201, 1021) m = multiple (general) 2i,4o means two inner arms, four outer arms, etc. --- N Number of measurements per item --- blank Blank (columns past here for R2 arcmin component of R1R2 arcmin cases ONLY) --- RAh2 Right Ascension 1950 (hours) h RAm2 Right Ascension 1950 (minutes) min RAs2 Right Ascension 1950 (seconds) s DE-2 Declination 1950 (sign) --- DEd2 Declination 1950 (degrees) deg DEm2 Declination 1950 (minutes) arcmin Name2 Object Name --- O2 Outer feature classification --- F2 Family classification --- I2 Inner feature classification --- T2 Numerical stage index (RC3 scale) --- u_T2 Uncertainty on T index --- D(O)2 Outer feature major axis diameter arcmin u_D(O)2 Uncertainty on D(O)2 --- d(O)2 Outer feature minor axis diameter arcmin u_d(O)2 Uncertainty on d(O)2 --- The(O)2 Relative bar/outer feature major axis position angle deg u_The(O)2 Uncertainty on The(O)2 --- o_O No. of outer feature classifications --- o_Family No. of family classifications --- o_I No. of inner feature (variety) classifications --- o_T No. of stage classifications --- o_D(O) No. of outer feature major-axis diameter estimates --- o_d(O) No. of outer feature minor-axis diameter estimates --- o_Thet(O) No. of estimates of rel. bar, outer feature major-axis position angle --- o_D(I) No. of inner feature major-axis diameter estimates --- o_d(I) No. of inner feature minor-axis diameter estimates --- o_Thet(I) No. of estimates of rel. bar, inner feature major-axis position angle --- Notes to Catalog RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Name Object Name --- Field SRC-J, ESO-B, or ESO-R field number --- Notes Description of object --- Additional Classified Galaxies RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin Name Object Name --- Special Special feature L refers to outer lens PR refers to polar ring Xg refers to X-shaped galaxy --- Family Family or class SX- means SAB with A underlined; SX means SAB with no underlines; and SX+ means SAB with B underlined E refers to elliptical I refers to irregular --- Variety Variety rs+ means rs with s underlined l refers to inner lens --- Stage Revised Hubble stage --- Peculiar Symbol for peculiarities --- T Numerical stage index Numerical stage index on scale of Third Reference Catalogue of Bright Galaxies (de Vaucouleurs et al. 1991, Springer: New York) --- u_T Uncertainty symbol for T --- Mult Multiplicity of outer spiral pattern Number of spiral arms n+ means n or more arms f means flocculent (see Elmegreen and Elmegreen, 1982, MNRAS< 201, 1021) m = multiple (general) 2i,4o means two inner arms, four outer arms --- Nancy G. Roman SSDOO/ADC 1995 Aug 11 The data and this document were submitted by Ronald J. Buta on July 3, 1995. We thank him for this cooperation and also for his help in correcting a few problems. The catalog was reformatted to eliminate unnecessary blank spaces and the document modified somewhat by the undersigned. J_ApJS_96_39.xml A Catalog of Far-Ultraviolet Point Sources Detected with the FAUST Telescope on ATLAS-1 J/ApJS/96/461 J/ApJS/96/461 Far-UV Point Sources A Catalog of Far-Ultraviolet Point Sources Detected with the FAUST Telescope on ATLAS-1 S Bowyer T P Sasseen X Wu M Lampton Astrophys. J. Suppl. Ser. 96 461 1995 1995ApJS...96..461B Photometry, ultraviolet Spectrophotometry catalogs techniques: photometric ultraviolet: galaxies ultraviolet: stars We list the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4698 Galactic and extragalactic objects detected in 22 wide-field images of the sky. At the locations surveyed, this catalog reaches a limiting magnitude approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14^ ergs/s/cm2/A, although it is not complete to this level. We list for each object the position, FUV flux, the error in flux, and where possible an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD, SAO, the HIPPARCOS Input Catalog, the Position and Proper Motion Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. We identify 2239 FAUST sources with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. We estimate the number of sources with incorrect identifications to be less than 2%. The experiment, the mission and the data are described in a previous paper by Bowyer et al., 1993ApJ...415..875B .
FAUST
List of FAUST sources FAUST Entry in FAUST catalog --- RAh Right ascension (1950) h RAm R.A. min RAs R.A. s DE- Declination sign --- DEd Declination (1950) deg DEm Dec. arcmin Flux Flux (photons/s/cm2/Angstroem) 10ct/s/cm2/nm e_Flux Uncertainty in flux 10ct/s/cm2/nm Dist Distance to catalog object Quantities are taken from the MHD catalog if a star is present. If an MHD star is not present, these quantities are taken (in order of preference) from the HIC, PPM, SAO, and HD catalogs. arcmin Vmag V magnitude of star mag Sp Spectral type --- HD HD or MHD catalog number <III/135> --- HIC Hipparcos Input Catalog <I/196> --- PPM PPM Catalog number <I/146> <I/193> These numbers do not agree with the catalogues <I/193> (Southern part of PPM) and <II/59> (TD1 catalogue) --- SAO SAO Catalog number <I/131> or McCook & Sion Catalog number <III/129> (shown in parentheses) --- TD1 TD1 Catalog number <II/59> --- GalDist Distance to galaxy, if present arcmin GalName Galaxy name --- CDS 1995 Jul 12 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 08-May-95 J_ApJS_96_461.xml Far-Ultraviolet Stellar Photometry: Fields in Sagittarius and Scorpius J/ApJS/96/605 J/ApJS/96/605 Far UV Stellar Photometry Far-Ultraviolet Stellar Photometry: Fields in Sagittarius and Scorpius E G Schmidt G R Carruthers Astrophys. J. Suppl. Ser. 96 605 1995 1995ApJS...96..605S Photometry, ultraviolet Stars, early-type stars: early-type surveys techniques: photometric ultraviolet: stars Far-ultraviolet photometry for 741 objects in a field in Sagittarius centered near M8 and 541 objects in a field centered near zeta Scorpii is presented. These data were extracted from electrographic images obtained with two cameras during a shuttle flight in 1991 April/May. The cameras provided band passes with lambda_eff = 1375 A and lambda_eff = 1781 A. Synthetic colors show that these bands are sensitive to effective temperature for hot stars. Our measurements were placed on a quantitative far-ultraviolet magnitude scale by convolving the spectra of stars observed by IUE with our cameras' spectral response functions. Fifty-eight percent of the ultraviolet objects were identified with visible stars using the SIMBAD database while another 40% of the objects are blends of early type stars too close together to separate with our resolution. Our photometry is compared with that from the TD-1, OAO 2, and ANS satellites and the S201 (Apollo 16) far-ultraviolet camera and found to agree at the level of a few tenths of a magnitude. Unlike previous studies, almost half of the identified visual counterparts to the ultraviolet objects are early B stars. A plot of distance modulus against ultraviolet color excess reveals a significant population of stars with strong ultraviolet excesses.
*Ultraviolet objects in the M8 field *Ultraviolet objects in the zeta Sco field Star Star number --- RAh Right ascension (1950) the printed values are all missing the '1' (e.g. ' 7' instead of '17') h RAm R.A. min RAs R.A. s DE- Declination sign --- DEd Declination (1950) deg DEm Dec. arcmin m1375 Magnitude at 1375 Angstroems mag m1781 Magnitude at 1781 Angstroems mag ID Identification --- Mag V or ptg. magnitude from SIMBAD mag n_Mag 'P' when Mag is photographic --- Sp Spectral type --- CDS 1995 Jul 12 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 08-May-95 UNKNOWN UNKNOWN * 12-Jul-1995: The original tables 4 and 5 where modified at CDS to place the magnitude flag 'P' in a dedicated column. * 05-Nov-1996: The RAh values were discovered to be wrong by 10 hours at CDS; all RAh values were then changed. J_ApJS_96_605.xml A multiparametric analysis of the Einstein sample of early-type galaxies. I. Luminosity and ISM parameters. J/ApJS/97/141 J/ApJS/97/141 Einstein sample multiparametric analysis. I. A multiparametric analysis of the Einstein sample of early-type galaxies. I. Luminosity and ISM parameters. P B Eskridge G Fabbiano D -W Kim Astrophys. J. Suppl. Ser. 97 141 1995 1995ApJS...97..141E Galaxies, spectra galaxies: elliptical and lenticular, cD galaxies: general galaxies: ISM X-rays: galaxies We have conducted bivariate and multivariate statistical analysis of data measuring the luminosity and interstellar medium of the Einstein sample of early-type galaxies (presented by Fabbiano, Kim & Trinchiere =1992ApJS...80..531F).
Einstein
Flux Data Name Galaxy name --- BT0 B magnitude mag MType Morphological type --- log(a/b) Ratio of axes in log. scale --- l_FX Limit flag on FX --- FX X-ray flux number=1 The value listed as upper limits are 3{sigma}. 10-13mW/m2 e_FX rms uncertainty on FX 10-13mW/m2 Dist Distance Mpc F12 Flux at 12um mJy e_F12 rms uncertainty on F12 mJy F25 Flux at 25um mJy e_F25 rms uncertainty on F25 mJy F60 Flux at 60um mJy e_F60 rms uncertainty on F60 mJy F100 Flux at 100um mJy e_F100 rms uncertainty on F100 mJy u_F100 Uncertainty flag on F100 --- F6cm Flux at 6cm mJy e_F6cm rms uncertainty on F6cm mJy F6core Core radio flux mJy e_F6core rms uncertainty on F6core mJy l_FHI Limit flag on FHI --- FHI 21cm HI line flux number=1 The value listed as upper limits are 3{sigma}. Jy.km/s ulFHI Upper limit of 21cm HI line flux in mJy/channel mJy Ref References number=2 IRAS references: 1. Knapp et al., 1989 <J/ApJS/70/329> 2. Knapp et al., 1989, blended: NGC 2832 with NGC 2831 NGC 4638 with NGC 4637 NGC 6876 with NGC 6877 3. Not observed by IRAS - Lonsdale et al., 1985, cat. <VII/113> 4. Rice et al., 1988, cat. <VII/109> 5. Fullmer and Lonsdale 1989, cat. <VII/113> 6. Fullmer and Lonsdale 1989, blended: NGC 1510 with NGC 1512 NGC 2444 with NGC 2445 NGC 6027 in a Zwicky Group NGC 127, NGC 130 and NGC 128 7. Condon et al., 1991 <1991AJ....101..362C> 8. Haynes et al., 1990 <1990AJ.....99.1740H> 9. Vereshchagin et al. <1989AZh....66..527V> Radio continuum references:. 10. FGT (Fabbiano et al., <1989ApJ...347..127F>) 11. Roberts et al., <1991ApJS...75..751R> 12. Wrobel <1991AJ....101..127W> 13. Wrobel and Heeschen <1988ApJ...335..677W> 14. Ekers and Ekers <1973A&A....24..247E> 15. Fabbiano et al., <1987ApJ...312..111F> 16. Wright <1974MNRAS.167..273W> 17. Sulentic <1976ApJS...32..171S> 18. Hummel et al., <1984A&A...134..207H> 19. Haynes et al., 1975 20. Disney and Wall <1977MNRAS.179..235D> 21. Calvani et al. <1989AJ.....97.1319C> 22. Hummel et al. <1991A&AS...87..309H> 23. Condon et al. <1991AJ....101..362C> Radio core references:. 24. Bridle and Fomalont <1978AJ.....83..704B> 25. Wrobel and Heeschen <1984ApJ...287...41W> 26. Geldzahler and Fomalont <1978AJ.....83.1047G> 27. Killeen et al., <1988ApJ...325..180K> 28. Stanger and Warwick <1986MNRAS.220..363S> 29. Burns et al. <1983ApJ...273..128B> 30. Killeen et al., <1986ApJ...302..306K> 31. Birkinshaw and Davies <1985ApJ...291...32B> 32. Fabbiano et al. <1984ApJ...277..115F> 33. Feretti et al. <1984A&A...139...55F> 34. Wrobel and Heeschen <1991AJ....101..148W> 35. Bridle and Perley 1984 36. Impey and Gregorini, 1993, cat. <J/AJ/105/853> 37. Sadler et al. <1989MNRAS.240..591S> 38. Wilkinson et al. <1987MNRAS.224..895W> 39. Neff and Hutchings <1992AJ....103.1746N> 40. Ekers et al. <1989MNRAS.236..737E> HI references:. 41. Roberts et al. <1991ApJS...75..751R> 42. Huchtmeier and Richter 1989 43. Huchtmeier and Richter 1989: NGC 7236 blended with NGC 7237. 44. Eder et al. <1991AJ....102..572E> 45. van Gorkom et al. <1989AJ.....97..708V>: HI in absorption 46. Bottinelli et al., 1990, cat. <VII/136> --- Luminosity data Name Galaxy name --- log(LB) B luminosity 10-7W l_log(LX) Limit flag on log(LX) --- log(LX) X-ray luminosity 10-7W l_log(LX/LB) Limit flag on log(LX/LB) --- log(LX/LB) B versus X luminosity --- l_log(L12) Limit flag on log(L12) --- log(L12) 12um luminosity 10-7W l_log(L100) Limit flag on log(L100) --- log(L100) 100um luminosity 10-7W l_log(L6) Limit flag on log(L6) --- log(L6) 6cm luminosity 10-7W l_log(L6CO) Limit flag on log(L6CO) --- log(L6CO) Core radio luminosity 10-7W l_log(MHI) Limit flag on log(MHI) --- log(MHI) HI mass solMass tables.tex TeX version of tables 1 to 11 Patricia Bauer CDS 1996 Aug 09 Paul Eskridge, <paul@druid.astr.ua.edu> J_ApJS_97_141.xml The Hubble Space Telescope Quasar Absorption Line Key Project. X. Galactic H I 21 centimeter emission toward 143 quasars and active galactic nuclei. J/ApJS/97/1 J/ApJS/97/1 HST Quasar Absorption Line Key Project. X. The Hubble Space Telescope Quasar Absorption Line Key Project. X. Galactic H I 21 centimeter emission toward 143 quasars and active galactic nuclei. F J Lockman B D Savage Astrophys. J. Suppl. Ser. 97 1 1995 1995ApJS...97....1L H I data QSOs Radial velocities Redshifts galaxies: active Galaxy: halo ISM: clouds quasars: absorption lines radio lines: ISM Sensitive H I 21cm emission line spectra have been measured for the directions to 143 quasars and AGNs chosen from the observing lists for the HST Quasar Absorption Line Key Project. Narrow-band and wide-band data were obtained with the NRAO 43m radio telescope for each object. The narrow-band data have a velocity resolution of 1km/s, extend from -220 to +170km/s, and are corrected for stray 21cm radiation. The wide-band data have a resolution of 4km/s and extend from -1000 to +1000km/s. The data are important for the interpretation of ultraviolet absorption lines near zero redshift in Key Project spectra. Twenty-two percent of the quasars lie behind Galactic high-velocity H I clouds with |VLSR|>100km/s whose presence can increase the equivalent width of interstellar absorption lines significantly. This paper contains the emission spectra and measures of the H I velocities and column densities along the sight line to each quasar. We discuss how the measurements can be used to estimate the visual and ultraviolet extinction toward each quasar and to predict the approximate strength of the strong ultraviolet resonance lines of neutral gas species in the HST Key Project spectra.
HST
Objects, velocities, and column densities Name Object name --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination deg DEm Declination arcmin DEs Declination arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Vmag V magnitude mag z Redshift --- l_E(B-V) Limit flag on E(B-V) --- E(B-V) B-V colour excess mag V- Observed negative LSR velocity limit of HI emission km/s V+ Observed positive LSR velocity limit of HI emission km/s <V> Average LSR velocity of the HI emission km/s N(HI)i Integrated HI column density assuming the emission to be optically thin 10+19cm-2 N(HI)200 Integrated HI column density assuming a spin temperature of 200K 10+19cm-2 Note Notes number=1 1: Quasar lies on or near an HVC listed in Table 3. 2: Wide-band or narrow-band HI measurements detect gas with |V_LSR_|>100km/s (see V- and V+ above and Table 2). 3: V-emission may extend to -85km/s (UM 341). 4: V+ includes HVC at 111.5km/s (PKS 1101-32). 5: Apparent emission extending to +80km/s probably not real (PKS 1103-00, MC 1104+167, and PKS 1424-11). 6: Apparent emission extending to 90km/s probably not real (B2 1208+32A). 7: Also has HVC at -207 and -198km/s (Mrk 205). 8: Emission wing extending to 50km/s probably not real (T 1542). 9: Emission may extend to 80km/s (PKS1252+11). 10: V- and V+ are averages of two observing sessions (NGC1275). 11: Possible emission to -120km/s (KAZ 102). 12: Because of the large value of T_b_(max), the line core can not be properly corrected for the effects of stray radiation. In Fig.1 we display the uncorrected data in the upper panel and the corrected data in the lower panel (PG 2112+059). 13: Emission may extend to -185km/s (3C 263.0). 14: Stray radiation removal process introduces emission near -90km/s (OJ 287). 15: Stray radiation removal process introduces emission near 60km/s (PG 1402+261). 16: Because of the large value of T_b_(max), the line core can not be properly corrected for the effects of stray radiation. The uncorrected data which are displayed in Fig.1 are reliable in the core but unreliable in the faint wings. The corrected data were used to derive V- and V+ (3C 120). 17: Site line intersects a molecular cloud. E(B-V) from H I is therefore a lower limit (3C 454.3). 18: Because of a telescope pointing error, the position actually observed (RA=11h19m10s9 and DE=12deg10'42") differs by approximately 10' from the correct position. --- James Marcout, Patricia Bauer CDS 1997 Mar 27 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_97_1.xml Automated Surface Photometry for the Coma Cluster Galaxies: The Catalog J/ApJS/97/77 J/ApJS/97/77 Catalog of Coma Cluster Galaxies Automated Surface Photometry for the Coma Cluster Galaxies: The Catalog M Doi M Fukugita S Okamura K Tarusawa Astrophys. J. Suppl. Ser. 97 77 1995 1995ApJS...97...77D galaxies: clusters: individual (Coma) galaxies: fundamental parameters galaxies: photometry A homogeneous photometry catalog is presented for 450 galaxies with B25.5 <= 16 mag located in the 9.8 x 9.8 deg region centred on the Coma Cluster. The catalog is based on photographic photometry using an automated surface photometry software for data reduction applied to B-band Schmidt plates. The catalog provides accurate positions, isophotal and total magnitudes, major and minor axes, and a few other photometric parameters including rudimentary morphology (early or late type).
Catalog Num Internal number [DFO95] --- CGCG Identification from CGCG <VII/4A> --- NGC_IC Identification from NGC/IC catalogs --- UGC Identification from UGC <VII/26D> --- cz Redshift from CfA redshift survey --- RAh Right ascension (1950.0) Accuracy of equatorial coordinates are 0.6 arcsec (rms). h RAm R.A. min RAs R.A. s DE- Declination sign, always blank --- DEd Declination (1950.0) deg DEm Dec. arcmin DEs Dec. arcsec Blend Deblending flag 'A' and 'M' denote that these galaxies are deblended either automatically or manually. Manual deblending was done, when topology of the overlapping objects does not allow a unique solution, or when blended images are so large or complex that the deblending procedure requires too much computer memory. Photometric parameters may not be accurate for galaxies with these flags. --- B25.5 Isophotal magnitude B25.5. The mean error is estimated to be 0.1 mag. mag Bt Total magnitude Bt The total magnitude is obtained by fitting the growth curve at the three faintest isophotal levels (dividing the intensity range between the peak and the threshold, 25.5 mag/s, into 20 levels) to the fiducial growth curves expected for the de Vaucouleurs profile (for E-type galaxies) and the exponential profile (for L-type galaxies), and then by reading the magnitude at 5 times the effective radius. For U-type galaxies, we average the two values obtained from the two profiles. Note that the definition of this total magnitude differs from that of BT (defined by RC2) commonly used in the literature; the offset between the two total magnitudes is found to be ~0.03 mag (Bt is brighter). When a good fit is not obtained for the three points, Bt is not listed. mag a Semimajor axis at 25.5 mag/arcsec2 Semimajor and semiminor axes at a surface brightness level of 25.5 mag/arcsec^2. 7-10% errors are expected for both parameters. arcsec b Semiminor axis at 25.5 mag/arcsec2 arcsec PA Position angle of major axis deg SB25.5 Mean surface brightness Mean surface brightness defined by equation (3) in the printed paper with muL = 25.5 mag/arcsec^2. mag cIndex Concentration index defined by Eq.2 in paper --- re25.5 Effective radius Effective radius that contains half the flux of B25.5. arcsec Type E=early, L=late, U=unclassified Morphology: 'E' (early, E-S0) or 'L' (late, Sa-Im), according to the criterion discussed in section 2 of the printed paper. The confidence level of the coincidence with RC3 morphology (early or late) is 87.5%. 'U' denotes a galaxy which is unclassified. --- Star Objects found to be blended stars The objects are marked by asterisks when they are classified as galaxies by the automated software, but turned out to be blended stars ("double" stars) upon visual inspection. --- CDS 1995 Jul 12 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 08-May-95 UNKNOWN UNKNOWN at CDS: The blank internal numbers in table1 (col. "Num") have been replaced by the actual number. J_ApJS_97_77.xml The First Caltech-Jodrell Bank VLBI survey. I. Lambda = 18 centimeter observations of 87 sources J/ApJS/98/1 J/ApJS/98/1 First Caltech-Jodrell Bank VLBI Survey. I. The First Caltech-Jodrell Bank VLBI survey. I. Lambda = 18 centimeter observations of 87 sources A G Polatidis P N Wilkinson W Xu A C S Readhead T J Pearson G B Taylor R C Vermeulen Astrophys. J. Suppl. Ser. 98 1 1995 1995ApJS...98....1P J/ApJS/98/33 : First Caltech-Jodrell Bank VLBI Survey. II (Thakkar+ 1995) J/ApJS/99/297 : First Caltech-Jodrell Bank VLBI Survey. III (Xu+ 1995) J/ApJS/95/345 : Second Caltech-Jodrell Bank VLBI Survey. I. (Taylor+ 1994) J/ApJS/100/1 : Second Caltech-Jodrell Bank VLBI Survey. II (Henstock+ 1995) QSOs Radio sources VLBI quasars: general radio continuum: galaxies surveys techniques: interferometric We present the first results from the first Caltech-Jodrell Bank VLBI survey (the CJ1 survey). The CJ1 sample includes 135 radio sources with total flux density 1.3Jy>S_6cm>=0.7Jy, declination delta_1950>=35deg, and Galactic latitude |b^II|>10deg. It extends the flux density limit of the complete "PR" sample studied by Pearson & Readhead from 1.3 to 0.7Jy and increases the total number of sources from 65 to 200. The complete survey includes VLBI images at both lambda-18 and 6cm of all objects in the extended sample that have cores strong enough to be mapped with the Mark II VLBI system. These images provide a large enough sample to study, for example, the variety of morphologies exhibited by compact radio sources, cosmological evolution, superluminal motion, and misalignment between parsec-scale and kiloparsec-scale radio structures. In this paper we present lambda-18cm VLBI observations of 56 CJ1 and 31 PR sources made in 1990-1991, including images of 82 sources. The observations were made with a "snapshot" technique in which each source was observed in three 20-30-minute scans using an array of 12-16 antennas. The images have resolution 3-10mas and dynamic range greater than 100:1. Later papers in the series will present the remaining lambda-18cm observations, the lambda-6cm observations, and the analysis and interpretation of the results.
The complete CJ1 sample CJ1 B1950 source name according to IAU convention --- RAh Right ascension, J2000.0 h RAm Right ascension, J2000.0 min RAs Right ascension, J2000.0 s DEd Declination, J2000.0 deg DEm Declination, J2000.0 arcmin DEs Declination, J2000.0 Positions specified with a precision of 0.01" are from the Jodrell Bank- VLA Astrometric Survey (Patnaik et al. 1992MNRAS.254..655P, Tables 2 and 4; and unpublished observations); the remaining positions have been compiled from a variety of publications via the NASA Extragalactic Database (NED). arcsec S11cm Total flux density at 11 cm Total flux density at 11cm from Pauliny-Toth et al. 1978AJ.....83..451P Jy S6cm Total flux density at 6 cm Total flux density at 6cm from Kuhr et al. 1981AJ.....86..854K Jy S2.8cm Total flux density at 2.8 cm Total flux density at 3.6cm from Kuhr et al. 1981AJ.....86..854K Jy ID Optical identification Optical identification: BL - BL Lac object; EF - Empty Field; G - Galaxy; Q - Quasar; SO - Stellar object. --- V Apparent V magnitude mag n_z 'f' - featureless spectrum, '>' - limit --- z Redshift See notes to Table 1 in the printed paper for references. --- OBSy Date of VLBI observations (year) yr OBSm Date of VLBI observations (month) --- n_OBSy Notes on observation date Parentheses indicate that the source was observed but not mapped; in three cases (marked with an asterisk) this is because the a priori position assumed for correlations was wrong, while in the other cases the source was too heavily resolved. A blank field indicates that the source was not observed because it does not contain a compact component strong enough for detection with Mark-II VLBI. --- r_OBS Reference to published observation 1: Xu et al. 1994AJ....108..395X 2: Stickel & Khuer 1994 <J/A+AS/103/349> 3: Stickel, Meisenheimer & Khuer 1994 <<J/A+AS/105/211> 4: Spinrad et al. 1985 <J/PASP/97/932> 5: Browne et al. 1993MNRAS.263L..32B 6: Henstock, Browne & Wilkinson 1995 <J/ApJS/100/1> 7: Jackson 1989 (Ph.D. thesis, Univ. of Manchester) 8: Palomar Observatory Sky Survey 9: Hewitt & Burbidge 1993 <VII/158> 10: Eckart et al. 1987A&AS...67..121E 11: Sanghera 1992 (Ph.D. thesis, Univ. of Manchester) 12: Fanti et al. 1985A&A...143..292F 13: Dallacasa et al. 1995A&A...295...27D 14: Foulsham 1989 (M.Sc. thesis, Univ. of Manchester) 15: Jones et al. 1986ApJ...305..684J 16: Dallacasa et al. 1990 (in Compact Steep-Spectrum and GHz-peaked Spectrum Radio Sources, ed. C. Fanti, D. Fanti. C.P. O'Dea & R.T. Schilizzi, Bologna: Consiglio Nazionale delle Ricerche, 77 17: Sanghera 1989 (M.Sc. thesis, Univ. of Manchester) 18: Lawrence, Zucker, Readhead, Unwin, Pearson & Xu, 1995, ApJS, submitted --- Sources from the PR sample observed at 18 cm CJ1 B1950 source name according to IAU convention --- RAh Right ascension, J2000.0 h RAm Right ascension, J2000.0 min RAs Right ascension, J2000.0 s DEd Declination, J2000.0 deg DEm Declination, J2000.0 arcmin DEs Declination, J2000.0 Positions specified with a precision of 0.01" are from the Jodrell Bank- VLA Astrometric Survey (Patnaik et al. 1992MNRAS.254..655P, Tables 2 and 4; and unpublished observations); the remaining positions have been compiled from a variety of publications via the NASA Extragalactic Database (NED). arcsec S11cm Total flux density at 11 cm Total flux density at 11cm from Pauliny-Toth et al. 1978AJ.....83..451P Jy S6cm Total flux density at 6 cm Total flux density at 6cm from Kuhr et al. 1981AJ.....86..854K Jy S2.8cm Total flux density at 2.8 cm Total flux density at 3.6cm from Kuhr et al. 1981AJ.....86..854K Jy ID Optical identification Optical identification: BL - BL Lac object; G - Galaxy; Q - Quasar --- Vmag Apparent V magnitude mag z Redshift from Lawrence et al. Lawrence, Zucker, Readhead, Unwin, Pearson & Xu, 1995, ApJS, submitted --- OBSy Date of VLBI observations (year) yr OBSm Date of VLBI observations (month) --- Map parameters CJ1 B1950 source name according to IAU convention --- OBSy Date of VLBI observation (year) yr OBSm Date of VLBI observation (month) --- Samp VLBI sample (CJ1 or PR) source belongs to --- a18cmn FWHM of major axis of the restoring beam mas b18cmn FWHM of minor axis of the restoring beam mas PA18cmn Position angle of major axis, north through east deg S18cmn Peak flux density, naturally weighted map Data are in mJy/beam mJy e_S18cmn Off source rms, naturally weighted map mJy a18cmt FWHM of major axis of tapered map restoring beam mas b18cmt FWHM of minor axis of tapered map restoring beam mas PA18cmt Position angle of major axis, N through E deg S18cmt Peak flux density, tapered map mJy e_S18cmt Off source rms, tapered map mJy Gaussian models CJ1 B1950 source name according to IAU convention --- S Flux density of component Jy Rad Radius of component Radius of component, measured from position of first component mas Theta Angle to component Angle to component, measured north through east from the position of the first component deg a FWHM of major axis of component mas b/a Axial ratio of major to minor axis, b/a --- Phi Position angle of major axis, north through east deg Chi2 Chi-squared between the model and the self-calibrated UV-data --- CDS 1996 Oct 14 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 10-May-95 J_ApJS_98_1.xml The First Caltech-Jodrell Bank VLBI Survey. II. Lambda = 18 Centimeter Observations of 25 Sources J/ApJS/98/33 J/ApJS/98/33 First Caltech-Jodrell Bank VLBI Survey. II. The First Caltech-Jodrell Bank VLBI Survey. II. Lambda = 18 Centimeter Observations of 25 Sources D D Thakkar W Xu A C S Readhead T J Pearson G B Taylor R C Vermeulen A G Polatidis P N Wilkinson Astrophys. J. Suppl. Ser. 98 33 1995 1995ApJS...98...33T J/ApJS/98/1 : First Caltech-Jodrell Bank VLBI Survey. I (Polatidis+ 1995) J/ApJS/99/297 : First Caltech-Jodrell Bank VLBI Survey. III (Xu+ 1995) J/ApJS/95/345 : Second Caltech-Jodrell Bank VLBI Survey. I. (Taylor+ 1994) J/ApJS/100/1 : Second Caltech-Jodrell Bank VLBI Survey. II (Henstock+ 1995) QSOs Radio sources VLBI quasars: general radio continuum: galaxies surveys techniques: interferometric We report lambda-18 cm VLBI observations made in 1991 September of a further 25 objects from the first Caltech-Jodrell Bank VLBI Survey (the CJ1 survey). The CJ1 sample is a complete, flux-density limited sample of 135 radio sources with total flux density at lambda-6cm between 0.7 and 1.3Jy. These observations complete the lambda-18cm part of the survey. Together with the results of Paper I (Polatidis et al., <J/ApJS/98/1>), we have now observed 81 CJ1 sources at lambda-18cm. Later papers in the series will present lambda-6cm observations and the analysis and interpretation of the results.
Map parameters CJ1 B1950 source name according to IAU convention --- OBSy Date of VLBI observation (year) yr OBSm Date of VLBI observation (year) --- Samp VLBI sample (CJ1 or PR) source belongs to --- a18cmn FWHM of major axis of the restoring beam mas b18cmn FWHM of minor axis of the restoring beam mas PA18cmn Position angle of major axis, north through east deg S18cmn Peak flux density, naturally weighted map Data are in mJy/beam mJy e_S18cmn Off source rms, naturally weighted map mJy a18cmt FWHM of major axis of tapered map restoring beam mas b18cmt FWHM of minor axis of tapered map restoring beam mas PA18cmt Position angle of major axis, N through E deg S18cmt Peak flux density, tapered map mJy e_S18cmt Off source rms, tapered map mJy Gaussian models CJ1 B1950 source name according to IAU convention --- S Flux density of component Jy Rad Radius of component Radius of component, measured from position of first component mas Theta Angle to component Angle to component, measured north through east from the position of the first component deg a FWHM of major axis of component mas b/a Axial ratio of major to minor axis, b/a --- Phi Position angle of major axis, north through east deg Chi2 Chi-squared between the model and the self-calibrated UV-data --- CDS 1996 Oct 14 AAS CD-ROM series, Volume 4, 1995 Lee Brotzman [ADS] 10-May-95 J_ApJS_98_33.xml A multifrequency radio continuum and IRAS faint source survey of Markarian galaxies J/ApJS/98/369 J/ApJS/98/369 Survey of Markarian galaxies A multifrequency radio continuum and IRAS faint source survey of Markarian galaxies M D Bicay G Kojoian J Seal D F Dickinson M A Malkan Astrophys. J. Suppl. Ser. 98 369 1995 1995ApJS...98..369B VII/172 : First Byurakan Survey (FBS) (Markarian+, 1989) Galaxies, IR Galaxies, Markarian Galaxies, radio galaxies: Seyfert galaxies: starburst infrared: galaxies radio continuum: galaxies surveys Results are presented from a multifrequency radio continuum survey of Markarian galaxies (MRKs) and are supplemented by IRAS infrared data from the Faint Source Survey. Radio data are presented for 899 MRKs observed at {nu}=4.755GHz with the NRAO-Green Bank 300 foot (91m) telescope, including nearly 88% of those objects in Markarian list VI-XIV. In addition, 1.415GHz measurements of 258 MRKs, over 30% of the MRKs accessible from NAIC-Arecibo, are reported. Radio continuum observations of smaller numbers of MRKs were made at 10.63GHz and at 23.1GHz and are also presented.
1.415 GHz and 4.755 GHz data Mrk Markarian number (Cat. <VII/172>) --- n_Mrk x: entry in the Appendix (appen file) --- n2_Mrk +: Additional radio continuum data (10.63GHx, 23.1GHz) listed in table3 --- Names Other names --- l_S1415MHz Limit flag on S1415MHz --- S1415MHz 1.415GHz flux density from NAIC-Arecibo mJy u_S1415MHz Uncertainty flag on S1415MHz --- e_S1415MHz rms uncertainty on S1415MHz mJy n_S1415MHz Note on S1415MHz number=1 a: Probable detection b: Possible detection; a weak signal, or unusual continuum profile c: Possible detection; confusion due to nearby objects and/or radio sources d: A hybrid b/c designation x: The detected signal is judged to not be associated with the MRK, but rather with a nearby source identified in the Appendix *: Not accessible from Arecibo Observatory --- obs1415MHz Number of useful radio continuum scans obtained at 1415MHz --- e1415MHz Number of separate observing runs during which the object was surveyed at 1415MHz --- logP1415 1.415GHz radio power [W/Hz] l_S4755MHz Limit flag on S4755MHz --- S4755MHz 4.755GHz flux density from NRAO-Green Bank mJy u_S4755MHz Uncertainty flag on S4755MHz --- e_S4755MHz rms uncertainty on S4755MHz mJy n_S4755MHz Note on S4755MHz --- obs4755MHz Number of useful radio continuum scans obtained at 4755MHz --- e4755MHz Number of separate observing runs during which the object was surveyed at 4755MHz --- u_obs4755MHz Unconsistent result from more than one continuum scan --- l_logP4755 Limit flag on logP4755 --- logP4755 4.755GHz radio power [W/Hz] SpClass Spectral classification --- Supplementary 1.415 GHz and 4.755 GHz data Mrk Markarian number (Cat. <VII/172>) --- S1415MHz 1.415GHz flux density from WB92 number=1 White and Becker, 1992ApJS...79..331W, Cat. <VIII/17> mJy logP1415 1.415GHz radio power from WB92 [W/Hz] S4755MHz 4.755GHz flux density from 87GB number=2 Gregory and Condon, 1991ApJS...75.1011G, Cat. <VIII/14> mJy e_S4755MHz rms uncertainty from 87GB mJy logP4755 4.755GHz radio power [W/Hz] 10.63 GHz and 23.1 GHz data Mrk Markarian number (Cat. <VII/172>) --- l_S10.63GHz Limit flag on S10.63GHz --- S10.63GHz 10.63GHz flux density from Algonquin Radio Observatory mJy e_S10.63GHz rms uncertainty on S10.63GHz mJy n_S10.63GHz Note on S10.63GHz number=1 a: Probable detection b: Possible detection; a weak signal, or unusual continuum profile c: Possible detection; confusion due to nearby objects and/or radio sources d: A hybrid b/c designation x: The detected signal is judged to not be associated with the MRK, but rather with a nearby source identified in the Appendix *: Not accessible from Arecibo Observatory --- obs10.63GHz Number of useful radio continuum scans obtained at 10.63 GHz --- e10.63GHz Number of separate observing runs during which the object was surveyed at 10.63GHz --- logP10.63GHz 10.63GHz radio power [W/Hz] l_S23.1GHz Limit flag on S10.63GHz --- S23.1GHz 23.1GHz flux density from Owens Valley Radio Observatory mJy e_S23.1GHz rms uncertainty on S23.1GHz mJy n_S23.1GHz Note on S10.63Hz number=1 a: Probable detection b: Possible detection; a weak signal, or unusual continuum profile c: Possible detection; confusion due to nearby objects and/or radio sources d: A hybrid b/c designation x: The detected signal is judged to not be associated with the MRK, but rather with a nearby source identified in the Appendix *: Not accessible from Arecibo Observatory --- obs23.1GHz Number of useful radio continuum scans obtained at 23.1GHz --- e23.1GHz Number of separate observing runs during which the object was surveyed at 23.1GHz --- logP23.1GHz 23.1GHz radio power [W/Hz] Radio Spectral Indices Mrk Markarian number (Cat. <VII/172>) --- SI1 1.415GHz to 4.755GHz spectral index --- e_SI1 rms uncertainty on SI1 --- SI2 2.695GHz to 4.755GHz spectral index --- e_SI2 rms uncertainty on SI2 --- SI3 4.755GHz to 10.63GHz spectral index --- e_SI3 rms uncertainty on SI3 --- SI4 4.755GHz to 23.1GHz spectral index --- e_SI4 rms uncertainty on SI4 --- Appendix Mrk Markarian number (Cat. <VII/172>) --- --- --- Mrk2 Second Markarian number when pair --- Com Comments --- Patrica Bauer CDS 1997 Jun 06 Tables 2,3 and 4 were provided by M. Bicay in Mac binary format. Thanks to Marcus de Deus Silva for his help through BinHex and Excel... Aligned and reformatted by H.Andernach Feb.96 The appendix was prepared via OCR at CDS. J_ApJS_98_369.xml Ultraviolet and optical observations of OB associations in M31 J/ApJS/98/595 J/ApJS/98/595 OB associations in M31 Ultraviolet and optical observations of OB associations in M31 J K Hill J E Isensee R C Bohlin K -P Cheng P M N Hintzen R W OConnell M S Roberts A M Smith E P Smith T P Stecher Astrophys. J. Suppl. Ser. 98 595 1995 1995ApJS...98..595H Galaxies, photometry Photometry, ultraviolet galaxies: individual (M 31) galaxies: photometry galaxies: star clusters ultraviolet: stars The 'figures' directory contain finding charts for the observed associations in Postscript format. Images of the central and southern parts of the local group Sb spiral galaxy M31 were obtained by the Ultraviolet Imaging Telescope during the Astro-1 Spacelab mission. Stellar photometry is obtained for 611 stars in 59 van den Bergh associations in the near-UV A1 band (central wavelength 2490A), and for 130 of these stars in the far-UV B1 band (central wavelength 1520A). In addition, B-band magnitudes for 456 of the stars in ~30 associations, together with U- and R-band photometry for ~290 stars in ~15 associations are determined from CCD images. B-magnitudes from the catalog of Magnier et al. (1992A&AS...96..379M) are given for 137 stars and R-magnitudes for 233 stars. Stellar positions are obtained from the ground-based CCD images and from UIT images. Total fluxes in the UV bands are measured for 63 associations. Finding charts are presented in the NUV and FUV bands, as well as one optical band. Tables give the images utilized in this investigation, the associations observed, with positions, total UV fluxes, extinctions estimated from color-magnitude diagrams, and stellar positions with photometry in up to five bands. UV color magnitude diagrams are presented with extinctions estimated by comparing the observed association color magnitude diagrams with colors and magnitudes of early-type stars computed from the IUE spectral atlas of Fanelli et al. (1992ApJS...82..197F). Comparison with evolutionary models suggests a maximum initial mass ~85M_{sun}_. Ultraviolet extinction within most M31 OB associations is found to follow an extinction curve similar to that of Hutchings et al. (1992ApJ...400L..35H). The variation in the fraction of near-UV stars also measured in the far-UV among the associations is probably caused by variations in age, extinction, and the degree of foreground contamination.
Positions of M31 associations and numbers of stars observed by UIT vdB van den Bergh association observed by UIT --- RAh Right Ascension, equinox J2000 h RAm Right Ascension, equinox J2000 min RAs Right Ascension, equinox J2000 s DE- Sign declination (always blank) --- DEd Declination, equinox J2000 deg DEm Declination, equinox J2000 arcmin DEs Declination, equinox J2000 arcsec N(NUV) No. of stars observed in near-UV (2490 A) --- N(FUV) No. of stars observed in far-UV (1520 A) --- Extinction and ultraviolet surface photometry of M31 associations vdB van den Bergh association observed by UIT --- E(B-V) Value of E(B-V) within M31 Value of E(B-V) within M31 estimated by comparing association CMDs with the library of Fanelli et al. (1992ApJS...82..197F). --- Z249 Normalized extinction Z249 = A249/E(B-V) --- Z152 Normalized extinction Z152 = A152/E(B-V) --- l_f249 f249 limiting characters, '>=' --- f249 Near-UV total flux above the sky Total flux and fractional error above the sky in the near-UV A1 band (central wavelength 2490A), in units of 10E-14ergs/cm^2/A/s. --- e_f249 fractional error in f249 --- l_f152 f152 limiting characters, '>=' --- f152 Far-UV total flux above the sky Total flux and fractional error above the sky in the near-UV B1 band (central wavelength 1520A), in units of 10E-14ergs/cm^2/A/s. --- e_f152 Fractional error in f152 --- m152-m249 m152-m249 = -2.5xlogf152/f249 mag T249 Fraction of f249 by nonforeground stars The flux contributed in the near-UV by stars thought to be galactic foreground stars has been subtracted from the total near-UV flux for the association. Foreground stars are generally not measurable in the far-UV. Total fluxes of the associations in the UIT bands are computed from the areas outlined on the charts. Sky values are estimated from the average of several nearby approximately circular areas of ~10" diameter. The fractions of the total flux in the UIT bands contributed by the measured nonforeground stars are given. --- T152 Fraction of f152 by nonforeground stars --- Source identifications, positions and magnitudes vdB van den Bergh association observed by UIT No stars are measurable in the UIT bands in four faint associations. --- n_vdB Always '-', separating assoc. and seq. nos. --- Seq Sequential number of star within association --- Xpos X offset E of N of fiducial pos. in Table 2 arcsec Ypos Y offset E of N of fiducial pos. in Table 2 arcsec m249 Near-UV magnitude mag m152 Far-UV magnitude mag Umag U magnitude mag Bmag B magnitude mag Rmag R magnitude mag ID Alternate identification Sources identified with open clusters (Hodge 1979AJ.....84..744H) or globular clusters (Bohlin et al. 1993ApJ...417..127B) are noted in this field. Stars measured in A78 corresponding with stars in field 1 of Massey, Armandroff, & Conti (1986AJ.....92.1303M) are also noted. Stars identifiable with stars in the catalog of Magnier et al. (1992A&AS...96..379M) are noted by Mn, where n is the Magnier identification number. Where possible, table 4 contains magnitudes obtained from the authors' B and R images. When a star has a Magnier number, but the B (or R) magnitude is from the author's data, as asterisk (or plus sign) appears after the Magnier number in Table 4. Probable foreground stars are designated by an "F". --- table2.tex LaTeX version of table2.dat table3.tex LaTeX version of table3 table4.tex LaTeX version of table4.dat environ.tex Custom LaTeX environments and related macros UNKNOWN 1996 Feb 01 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 02-Aug-95 J_ApJS_98_595.xml A statistical distance scale for galactic planetary nebulae J/ApJS/98/659 J/ApJS/98/659 Galactic PNe statistical distance scale A statistical distance scale for galactic planetary nebulae C Y Zhang Astrophys. J. Suppl. Ser. 98 659 1995 1995ApJS...98..659Z V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+ 1992) Aaquist & Kwok, 1990 A&AS 84, 229 =1990A&AS...84..229A Cahn et al., 1992 A&AS 94, 399 =1992A&AS...94..399C Milne, 1979 A&AS 36, 227 =1979A&AS...36..227M Milne & Aller, 1975 A&A 38, 183 =1975A&A....38..183M Pottasch, 1984 Planetary nebulae (Dordrecht: Reidel) Pottasch & Zijlstra, 1994 A&A 289, 261 =1994A&A...289..261P Roelfsema et al., 1991 A&A 251, 611 =1991A&A...251..611R Van de Steene and Zijlstra, 1994, =1994A&AS..108..485V Van de Steene and Zijlstra, 1995, A&A 293, 541 =1995A&A...293..541V Zijlstra et al., 1989 A&AS 79, 329 =1989A&AS...79..329Z Planetary nebulae Stars, distances distance scale planetary nebulae: general A statistical distance scale is proposed. It is based on the correlation between the ionized mass and the radius and the correlation between the radio continuum surface brightness temperature and the nebular radius. The proposed statistical distance scale is an average of the two distances obtained using the correlations. These correlations, calibrated on the 132 planetary nebulae with well-determined individual distances by Zhang, can reproduce not only the average distance of a sample of Galactic Bulge planetary nebulae exactly at the distance to the Galactic center, but also the expected gaussian distribution of their distances around the Galactic center. This new distance scale is applied to 647 Galactic planetary nebulae. It is estimated that this distance scale can be accurate on average to 35%-50%. Our statistical distance scale is in good agreement with the one recently proposed by Van de Steene and Zijlstra
Planetary nebulae with individually determined distances Name Common name --- PK Perek & Kohoutek name --- Dist Individually determined distance kpc S5GHz 5 GHz (6 cm) radio flux density mJy Diam Diameter of nebula arcsec Tb Radio Brightness Temperature K Rad Radius of nebula pc Mi Ionized gas mass of nebula solMass DMi Statistical distance derived from mass-radius relation kpc DTb Statistical distance from Tb - R relation kpc Df Mean of DMi and DTb adopted as final result number=1 In Table 1 of the paper, Dm should read Df. kpc Delta Fractional difference between Df and Dist % Catalog of statistical distances of planetary nebulae Name Common name --- PK PK name --- S5GHz 5 GHz (6 cm) radio flux density mJy Diam Diameter of nebula in arcsec arcsec Ref References for the previous columns number=1 Reference numbers are: 1: Pottasch (1994A&A...289..261P) 2: Aaquist & Kwok (1990A&AS...84..229A) 3: Zijlstra et al. (1989A&AS...79..329Z) 4: Milne & Aller (1975A&A....38..183M) 5: Milne (1979A&AS...36..227M) 6: Roelfsema et al. (1991A&A...251..611R) 7: Cahn et al. (1992A&AS...94..399C) 8: Pottasch & Zijlstra (1994A&A...289..261P) --- Tb Radio Brightness Temperature K DMi Statistical distance derived from mass-radius relation kpc DTb Statistical distance from Tb - R relation kpc Df Mean of DMi and DTb adopted as final result number=2 In Table 3 of the paper, Dm should read Df. kpc D(VSZ) Distance from Van de Steene and Zijstra (1995) kpc D(CKS) Distance from Cahn, Kaler & Stanghellini (1992) kpc table1.tex LaTeX version of table1 table3.tex LaTeX version of table3 Patricia Bauer CDS 1996 Aug 28 <zhang@iras.ucalgary.ca> J_ApJS_98_659.xml The Relation Between Rotational Velocities and Spectral Peculiarities Among A-Type Stars J/ApJS/99/135 J/ApJS/99/135 Rotation and Spectral Peculiarities The Relation Between Rotational Velocities and Spectral Peculiarities Among A-Type Stars H A Abt N I Morrell Astrophys. J. Suppl. Ser. 99 135 1995 1995ApJS...99..135A Equivalent widths Rotational velocities Stars, peculiar stars: chemically peculiar stars: early-type stars: fundamental parameters stars: rotation We obtained new data to determine whether the spectral appearance of A-type stars is entirely determined by their rotational velocities. For this purpose we derived rotational velocities for 1700 northern A-type stars from CCD coude spectra, calibrated with the new Slettebak et al. system, and new MK classifications based on wide photographic Cassegrain spectra for 2000 northern and some southern stars in the Bright Star Catalogue. In addition we determined the equivalent widths of the lambda 4481 Mg II lines in the coude spectra. Tables and graphs show variations of rotational velocities and lambda 4481 line strengths as functions of type and luminosity, and frequencies of the normal and abnormal stars. After deconvolutions of the rotational velocities, assuming random orientations of rotational axes, we find that all rapid rotators have normal spectra and nearly all slow rotators have abnormal spectra (Ap or Am). Those abnormalities are generally attributed to diffusion and can occur only with little rotational mixing. However at all types there are overlaps of these distributions, implying that a given intermediate rotational velocity is insufficient to determine whether the star should have a normal or abnormal spectrum. However, we realized that (1) some of our "standards," such as Vega and Alpha Dra, are really abnormal, causing us to classify similar peculiar stars as "normal," (2) many of the "normal" stars near A2 IV have the characteristics of peculiar stars such as low rotational velocities and weak 4481 Mg II and K lines, and (3) the mean rotational velocities of "normal" stars are depressed just at those types where the Ap and Am stars are most frequent. Therefore we conclude that the overlaps are due to our failure to detect all the abnormal stars and that a specific rotational velocity is probably enough to determine whether a star will have a normal or abnormal spectrum.
Summary of Stellar Data HR Bright Star Catalogue number If both the HR and HD fields are blank, the remaining fields are continuations of the previous record. --- HD Henry Draper or Aitken Double Star number --- MK MK classification Explanation of the Classification Terminology (from Table 1): (standard) Classification standard star s Sharp lined n Broad lined nn Very broad lined ksn The Ca II K line has both sharp and broad components st Strong wk Weak v. Very Lam Boo A star in which many of the metals are weak, indicating underabundances 4481 weak The 4481 Mg II line is weak. Measures may indicate that other lines are also weak. This may be a mild version of the Lambda Boo stars. Am(A3/A7/F0) A metallic line star in which the spectral type based on the Ca II K line is A3, on the Balmer lines is A7, and on the metallic lines is F0. This is an abbreviation of the form Am(K/H/M=A3/A7/F0). p(SrEuCr st, CaMg wk) An Ap star in which the Sr is strongest relative to the standards, Eu is next strongest, etc.; the lines of Ca and Mg are weak relative to those in standards. The type is based on the hydrogen lines. shell(Ti,Ca) A shell spectrum that has sharp Ti and Ca absorption lines. (:) Uncertainty in the previous symbol. --- l_Vsini Limiting character on Vsini --- Vsini Vsini, rotational velocity km/s u_Vsini Vsini uncertainty flag Uncertainty flag, or indication if this is a program star (p) or a star from Slettebak et al. (1975ApJS...29..137S) --- W4481 Equivalent width for 4481 A line 0.1nm u_W4481 W4481 uncertainty flag --- CDS 1996 Feb 01 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 02-Aug-95 J_ApJS_99_135.xml Atlas of synthetic ultraviolet spectra of massive star populations J/ApJS/99/173 J/ApJS/99/173 Synthetic UV spectra of massive stars Atlas of synthetic ultraviolet spectra of massive star populations C Leitherer C Robert T M Heckman Astrophys. J. Suppl. Ser. 99 173 1995 1995ApJS...99..173L Spectra, ultraviolet Stars, early-type atlases stars: early-type stars: mass-loss stars: Wolf-Rayet ultraviolet: stars An atlas of synthetic ultraviolet spectra of a population of massive stars is presented. The spectra are based on a stellar library of IUE high-dispersion spectra of O and Wolf-Rayet stars, coupled to an evolutionary synthesis code. Later spectral types are included via low-dispersion spectra. Line profiles of N V lambda 1240, Si IV lambda 1400, C IV lambda 1550, He II lambda 1640, and N IV lambda 1720 have been computed for star-formation histories and initial mass functions typically found in starburst regions. It is found that the lines are sensitive indicators for the presence or absence of massive stars. C IV lambda 1550 is the strongest stellar line in the ultraviolet spectrum of a typical starburst. If O stars with zero-age main-sequence masses above 50M_{sun}_ are present, C IV always shows a P Cygni profile. In the absence of such stars, only a blue-shifted absorption is present. During later epochs of the starburst, when late-O/early-B stars dominate, an unshifted photospheric absorption appears. Si IV lambda 1400 shows a conspicuous wind profile when luminous O supergiants are present. A strong P Cygni profile is found only for an instantaneous burst observed at 3 to 5Myr, which has a top-heavy IMF. The velocity of the blueshifted absorption is strongly correlated with the age and the upper cutoff mass (or slope) of the IMF. N V lambda 1240 traces the most massive stars and behaves rather similar to Si IV lambda 1400. Its usefulness as an indicator of very massive stars is limited due to the strong blending effect of the nearby Ly-alpha line. Nevertheless, strong N V lambda 1240 emission in a starburst suggests the presence of stars with masses in excess of 60M_{sun}_. He II lambda 1640 and N IV lambda 1720 are produced by very hot and luminous O and Wolf-Rayet stars. Both lines can have weak absorption or emission in a typical starburst but are predicted to be observable only under rare circumstances, such as in an instantaneous burst at t{approx.}3Myr. The profiles presented in the atlas can be compared to high-quality ultraviolet observations of galaxies with active star formation in order to constrain the massive star population. The atlas is published in its entirety in computer-readable form in the AAS CD-ROM series, Vol. 5.
*Spectra for 144 models Form b: burst star formation c: continuous star formation --- IMF IMF exponents (1.50, 2.35, 3.00 or 3.75) --- Mass Upper cut-off mass (30, 40, 60, 80 or 100 M_{sun}_) solMass Age Age, in intervals of 1.0 Myr Myr Lambda Wavelength 0.1nm log(Lum) Luminosity per wavelength interval (erg/s/A) uW/nm Spectrum Normalized spectrum, which is plotted in the figures in the printed paper. --- CDS 1996 Feb 01 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 29-Aug-95 J_ApJS_99_173.xml The First Caltech-Jodrell Bank VLBI Survey. III. VLBI and Merlin Observations at 5 GHz and VLA Observations at 1.4 GHz J/ApJS/99/297 J/ApJS/99/297 First Caltech-Jodrell Bank VLBI Survey. III The First Caltech-Jodrell Bank VLBI Survey. III. VLBI and Merlin Observations at 5 GHz and VLA Observations at 1.4 GHz W Xu A C S Readhead T J Pearson A G Polatidis P N Wilkinson Astrophys. J. Suppl. Ser. 99 297 1995 1995ApJS...99..297X J/ApJS/98/1 : First Caltech-Jodrell Bank VLBI Survey. I (Polatidis+ 1995) J/ApJS/98/33 : First Caltech-Jodrell Bank VLBI Survey. II (Thakkar+ 1995) J/ApJS/95/345 : Second Caltech-Jodrell Bank VLBI Survey. I. (Taylor+ 1994) J/ApJS/100/1 : Second Caltech-Jodrell Bank VLBI Survey. II (Henstock+ 1995) QSOs Radio sources VLBI quasars: general radio continuum: galaxies surveys We present the 5GHz results from the first Caltech-Jodrell Bank (CJ1) VLBI survey. The 1.6GHz maps were presented in two separate papers, Polatidis et al. <J/ApJS/98/1> and Thakkar et al. <J/ApJS/98/33>. These three papers complete the first stage of this program to map at both 1.6 and 5GHz all objects accessible to Mark II VLBI in the complete sample of 135 objects with 1.3>S(5Ghz)>=0.7Jy, Dec(1950)>=35deg, and |b|>10deg. The combination of the CJ1 sample with the Pearson-Readhead (PR) sample provides a complete, flux density-limited sample of 200 objects with S(5GHz)>=0.7Jy, Dec(1950)>=35deg, |b|>10deg for which all of the objects accessible to Mark II VLBI have been mapped at both 5GHz (129 objects) and 1.6GHz (132 objects). In addition to the 5GHz VLBI maps, we present in this paper 5GHz MERLIN observations of 20 objects and 1.4GHz VLA observations of 92 objects in the combined CJ1 + PR sample. The VLA maps, together with L-band (1.3-1.7GHz) maps available in the literature, provide a complete set of VLA maps for the combined CJ1 + PR sample. Finally, we present the radio spectra of the objects in the CJ1 sample. The combined CJ1 + PR VLBI surveys provide a sample which is large enough for a number of important astrophysical and cosmological studies. These will be presented in further papers in this series.
VLBI (5GHz) map parameters CJ1 B1950 source name, IAU convention --- OBSy Date of the VLBI observations (year) yr OBSm Date of the VLBI observations (month) --- Sample VLBI sample (CJ1 or PR) the source belongs to --- a5GHzn FWHM of major axis of the restoring beam mas b5GHzn FWHM of minor axis of the restoring beam mas PA5GHzn Position angle of major axis, N through E deg S5GHzn Peak flux density, naturally weighted map mJy e_S5GHzn Off source rms, naturally weighted map mJy a5GHzt FWHM of major axis of tapered map restoring beam mas b5GHzt FWHM of minor axis of tapered map restoring beam mas PA5GHzt Position angle of major axis, N through E deg S5GHzt Peak flux density, tapered map mJy e_S5GHzt Off source rms, tapered map mJy Gaussian models CJ1 B1950 source name according to IAU convention --- S Flux density of component Jy Rad Radius of component Radius of component, measured from position of the first component mas Theta Angle to component Angle to component measured north through east from the position of the first component deg a FWHM of major axis of component mas b/a Axial ratio of major to minor axis, b/a --- Phi Position angle of major axis, north through east deg Amp Amplitude agreement factor --- CP Closure Phase agreement factor --- Tot Total agreement factor --- MERLIN (5GHz) map parameters CJ1 Source name --- Sample Sample, CJ1 or PR --- a Beam FWHM major axis mas b Beam FWHM minor axis mas Theta Beam major axis position angle deg S5GHz Peak intensity mJy e_S5GHz rms noise mJy VLA (1.4GHz) map parameters Source Source name --- Sample Sample, CJ1 or PR --- S5GHz Peak intensity mJy e_S5GHz rms noise mJy Struct Structure Structure: U - unresolved E - extended structure detected E? - hint of extended structure Note flag: a Faint component ~ 12" to the north b Faint component ~ 1' to the west c Logarithmic contour levels in steps of 2^{1/2} d Convolved with 3" circular Gaussian beam e Convolved with 5" circular Gaussian beam f The lowest contour in 2 sigma g The lowest contour is 4 sigma h Source resolved at long baselines --- CDS 1996 Feb 02 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 29-Aug-95 UNKNOWN UNKNOWN All the figures are available on the AAS CD-ROM, directories: /volume5/apjs/v99/p297/figure2 /volume5/apjs/v99/p297/figure4 /volume5/apjs/v99/p297/figure6 J_ApJS_99_297.xml The CfA redshift survey: data for the NGP +36 zone. J/ApJS/99/391 J/ApJS/99/391 The CfA redshift survey: NGP +36 zone. The CfA redshift survey: data for the NGP +36 zone. J P Huchra M J Geller H G Corwin Jr. Astrophys. J. Suppl. Ser. 99 391 1995 1995ApJS...99..391H VII/164 : The CfA Redshift Catalogue, Version Nov. 1993 (Huchra+, 1993) Huchra 1976 AJ, 81, 952 Nilson 1973 UGC Catalogue <VII/26> Zwicky et al., 1961-1968 CGCG Catalogue <VII/49> Galaxy catalogs Redshifts galaxies: distances and redshifts galaxies: fundamental parameters surveys We have assembled redshifts for a complete sample of 719 galaxies with m_Zw_<=15.5 in the declination range 32.5deg<=delta<=38.5deg and right ascension range 8h<=alpha<=17h. We have determined morphological types for all galaxies in the magnitude limited sample by direct inspection of the POSS-O plates. 576 of the redshifts are measurements from Mount Hopkins, and 405 are new redshifts. We also include new redshifts for 77 fainter galaxies in the same strip.
CfA survey radial velocities Name IAU name of the Galaxy --- m_Name Multiplicity index on Name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec mag Apparent blue magnitude number=1 Apparent blue magnitude on the Zwicky-B(0) system (Huchra 1976); magnitudes from sources other than the Zwicky-Nilson merged catalog (Zwicky et al., 1961-1968 plus Nilson 1973) or the RC1 are noted, as are the split magnitudes for multiple objects. mag HRV Heliocentric radial velocity km/s e_HRV rms uncertainty on HRV km/s r_HRV Velocity source --- Type Numerically coded, revised Hubble type --- D1 Major axis diameter from the UGC --- D2 Minor axis diameter from the UGC --- BT Total B magnitude --- UGC UGC designation --- m_UGC Multiplicity index on UGC --- RFN RFN --- Com Comments and other names --- Patricia Bauer CDS 1996 Aug 26 We thank John Huchra <huchra@fang.harvard.edu> for kindly providing the data. J_ApJS_99_391.xml Rotation curves of 967 spiral galaxies J/ApJS/99/501 J/ApJS/99/501 Spiral galaxies rotation curves Rotation curves of 967 spiral galaxies M Persic P Salucci Astrophys. J. Suppl. Ser. 99 501 1995 1995ApJS...99..501P ftp://galileo.sissa.it/ftp/pub/psrot : (???) Galaxies, rotation catalogs galaxies: kinematics and dynamics galaxies: spiral We present the rotation curves of 967 southern spiral galaxies, obtained by deprojecting and folding the raw H{alpha} data originally published by Mathewson, Ford, & Buchhorn (1992ApJS...81..413M). For 900 objects, we also present, in figures and tables, the rotation curves smoothed on scales corresponding to 5%-20% of the optical size; of these, 80 meet objective excellence criteria and are suitable for individual detailed mass modeling, while 820, individually less compelling mainly because of the moderate statistics and/or limited extension, are suitable for statistical studies. The remaining 67 curves suffer from severe asymmetries, small statistics, and large internal scatter that may largely limit their use in galaxy structure studies. The deprojected folded curves, the smoothed curves, and various related quantities are available via anonymous ftp at galileo.sissa.it in the directory /users/ftp/pub/psrot.
Kinematic quantities, radii, inclinations, and quality codes for sample galaxies Name Galaxy name --- a Offset of the kinematic center from the photometric center along the major axis, along with the inclination angle "i" arcsec Vsys Heliocentric systemic velocity km/s Ropt Optical radius arcsec i Inclination angle deg Class Subset number=1 Set A includes 80 rotation curves that are smooth and symmetric, have negligible rms internal error, extend to at least the optical radius, have high and homogeneous radial data coverage. Set B includes 820 rotation curves of good quality which, however, have some limitations, such has subsampling, limited extension (i.e. R(farthest)<3 disk length scales), moderate asymmetries, noncircular motions, or nonnegligible rms internal error. Set C includes 67 curves with severe global asymmetries, scanty sampling, very large rms internal scatter, and conspicuous noncircular motions. --- Estimated rotation velocities at various fractions of the optical radius for sample galaxies Name Galaxy name --- Vrot0.2 Rotation velocity at 0.2 optical radius km/s n_Vrot0.2 Note on Vrot0.2 number=1 A ')' indicates velocities that come from smooth eyeball interpolation/extrapolation of the data points, for cases when we have deemed such a procedure safe. --- Vrot0.4 Rotation velocity at 0.4 optical radius km/s n_Vrot0.4 Note on Vrot0.4 number=1 A ')' indicates velocities that come from smooth eyeball interpolation/extrapolation of the data points, for cases when we have deemed such a procedure safe. --- Vrot0.6 Rotation velocity at 0.6 optical radius km/s n_Vrot0.6 Note on Vrot0.6 number=1 A ')' indicates velocities that come from smooth eyeball interpolation/extrapolation of the data points, for cases when we have deemed such a procedure safe. --- Vrot0.8 Rotation velocity at 0.8 optical radius km/s n_Vrot0.8 Note on Vrot0.8 number=1 A ')' indicates velocities that come from smooth eyeball interpolation/extrapolation of the data points, for cases when we have deemed such a procedure safe. --- Vrot1.0 Rotation velocity at 1.0 optical radius km/s n_Vrot1.0 Note on Vrot1.0 number=1 A ')' indicates velocities that come from smooth eyeball interpolation/extrapolation of the data points, for cases when we have deemed such a procedure safe. --- Vrot1.2 Rotation velocity at 1.2 optical radius km/s n_Vrot1.2 Note on Vrot1.2 number=1 A ')' indicates velocities that come from smooth eyeball interpolation/extrapolation of the data points, for cases when we have deemed such a procedure safe. --- Vrot1.4 Rotation velocity at 1.4 optical radius km/s n_Vrot1.4 Note on Vrot1.4 number=1 A ')' indicates velocities that come from smooth eyeball interpolation/extrapolation of the data points, for cases when we have deemed such a procedure safe. --- Vrot1.6 Rotation velocity at 1.6 optical radius km/s n_Vrot1.6 Note on Vrot1.6 number=1 A ')' indicates velocities that come from smooth eyeball interpolation/extrapolation of the data points, for cases when we have deemed such a procedure safe. --- Vrot1.8 Rotation velocity at 1.8 optical radius km/s Vas Outermost estimated velocity number=2 Outermost estimated velocity (for radii>=1.0Ropt) as a representative measure of the galaxy asymptotic rotation velocity km/s Patricia Bauer CDS 1997 Dec 04 UNKNOWN UNKNOWN copied by ftp at galileo.sissa.it in the directory pub/psrot J_ApJS_99_501.xml The massive star populations in ionized gas shells in M33 and M31 J/ApJS/99/551 J/ApJS/99/551 BVI photometry of massive stars in M33 and M31 The massive star populations in ionized gas shells in M33 and M31 D A Hunter D M Boyd W N Hawley Astrophys. J. Suppl. Ser. 99 551 1995 1995ApJS...99..551H Interstellar medium Photometry galaxies: individual (M 31, M 33) galaxies: ISM galaxies: star clusters galaxies: stellar content stars: early-type We present BVI photometry of the massive stars in and around five Halpha shells in M33 and two in M31. These data can be used to statistically compare the stellar population with ionization and formation requirements of the gas shell. We have counted the numbers of massive stars encircled by the shells and embedded within the gaseous structures and corrected these numbers statistically for background and foreground interlopers. We find that the stellar production exceeds the ionization requirements of the nebulae by factors of 4-10. Thus, it is reasonable that the shells are photoionized and that a large fraction of the ionizing photons escape into the rest of the galaxy. We have also compared the number of massive stars counted and extrapolated to 7M_{sun}_ with the number required to form the shells according to a simple formation model. With one exception, we find that the number of stars estimated to be present exceeds the number required by the model for our assumptions of age and ambient gas density. This comparison and the morphology evident in Halpha images suggests that the modification of the interstellar medium by the massive stars in these regions has been far more complicated than is currently considered in formation models. There is evidence for multiple, and to some extent discreet, events in the production of the gas structures. A more detailed modeling will be necessary to adequately account for the stellar populations and Halpha morphology.
The photometry Region The region in M33 or M31 --- Group Group identification number within region See Table 3 for descriptions of the groups. --- Star Star identification number within the group --- Xpos X pixel coordinate The X,Y pixel coordinates are relative to the long V-band image shown in figure 1 (plates 11-16) of the printed paper. pix Ypos Y pixel coordinate pix Vmag V magnitude mag e_Vmag Uncertainty in V mag B-V B-V color A magnitude of 100.00 indicates that the star was not measured through that filter. mag e_B-V Uncertainty in B-V color mag V-I V-I color mag e_V-I Uncertainty in V-I color mag The groups and reddening Region The region in M33 or M31 --- Group Group identification number within region --- Comment Comment on the group --- E(B-V) Reddening --- CDS 1996 Feb 02 AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 31-Aug-95 J_ApJS_99_551.xml The EINSTEIN Extended medium sensitivity survey second epoch: results for the stars J/ApJS/99/701 J/ApJS/99/701 EMSS The EINSTEIN Extended medium sensitivity survey second epoch: results for the stars T A Fleming S Molendi T Maccacaro A Wolter Astrophys. J. Suppl. Ser. 99 701 1995 1995ApJS...99..701F IX/11 : ROSAT Source Catalog (Voges+ 1994) VII/152 : EINSTEIN Observatory Extended Medium-Sensitivity Survey (EMSS) X-ray sources stars: coronae surveys X-rays: stars We present X-ray data from the ROSAT all-sky survey for those sources catalogued in the Einstein Extended Medium Sensitivity Survey (EMSS) (Cat. <VII/152>) which have been identified with Galactic stars. This "second epoch" of X-ray data taken 10yr later, is used to study coronal flux variability for the most active examples of late-type stars. About 72% of the EMSS stars have been redetected by ROSAT. While the F-stars appear to have remained constant, we find evidence for a general decrease in X-ray flux for the M and solar-type stars. This is probably due to the fact that an X-ray-selected sample will preferentially detect stars while flaring. In contradiction to this, the RS CVn binaries have been redetected at higher X-ray flux levels for the sample as a whole.
ROSAT, Einstein
R0SAT PSPC survey data on all stars from the EMSS EMSS EMSS designation (See cat. <VII/152>) --- Type Stellar type number=1 Types B, A, F, G, K, M : spectral types BY : BY Dra binary CV : cataclysmic variable DA : white dwarf EW : W UMa binary FK : FK Com star PM : pre-main-sequence star RS : RS CVn binary --- l_ExpTime Limit flag on ExpTime --- ExpTime Total survey exposure time s n_ExpTime n: Not analysed --- l_RateTot Limit flag on RateTot --- RateTot Total corrected PSPC count rate number=2 For stars not detected, 3sigma upper limit ct/s n_RateTot *: Count rate computed manually --- e_RateTot 1-sigma error on RateTot ct/s l_RateHard Limit flag on RateHard --- RateHard Total corrected PSPC hard (0.5-2.0 keV) count rate ct/s e_RateHard 1-sigma error on RateHard ct/s HR Hardness ratio --- l_FluxTot Limit flag on FluxTot --- FluxTot Total flux (0.1-2.4 keV) (10^-13^erg/cm2/s) 10-16W/m2 l_FluxHard Limit flag on FluxHard --- FluxHard Hard flux (0.5-2.0 keV) (10^-13^erg/cm2/s) 10-16W/m2 James Marcout, Patricia Bauer CDS 1997 Feb 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_ApJS_99_701.xml Observations of Supernova Remnants at Pushchino: Catalog of Flux Densities at Meter Wavelengths. J/AZh/71/110 J/AZh/71/110 Supernova Remnants at Meter Wavelengths Observations of Supernova Remnants at Pushchino: Catalog of Flux Densities at Meter Wavelengths. A V Kovalenko A V Pynzar V A Udaltsov Astron. Zh. 71 110 1994 1994AZh....71..110K Radio sources Supernova remnants Surveys The total flux densities of more than one hundred galactic supernova remnants (SNR) at 111, 102, and 83MHz, measured at Pushchino using the E-W WBCR-1000 and LSA radio telescopes, to an accuracy of 2Jy or better; the spectral indices, with their errors, obtained from the compiled spectra; and optical depths at 100MHz in the direction of the supernova remnants are reported. The latter values are obtained from a low frequency cutoff caused by interstellar gas absorption, which was detected at meter and decimeter wavelengths in the direction of 38% of the supernova remnants.
Catalog of SNR Flux Densities at Meter Wavelengths GLON Galactic longitude deg GLAT Galactic latitude deg OtherNam Other Names of SNR --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin AS Angular size arcmin u_AS Uncertainty in size --- l_S83 Limit flag on S83 (> meaning >=) --- S83 Flux density at 83 MHz Jy e_S83 Mean error on S83 Jy l_S102 Limit flag on S102 (> meaning >=) --- S102 Flux density at 102 MHz Jy e_S102 Mean error on S102 Jy l_S111 Limit flag on S111 (> meaning >=) --- S111 Flux density at 111 MHz Jy e_S111 Mean error on S111 Jy l_alpha Limit flag on alpha (> meaning >=) --- alpha Spectral index --- e_alpha Mean error on alpha --- u_alpha Uncertainty on alpha --- S1 Flux density at 1 GHz Jy u_S1 Uncertainty on S1 --- l_Tau Limit flag on Tau (> meaning >=) --- Tau Optical depth at 100 MHz --- e_Tau Mean error on optical depth --- u_Tau Uncertainty on Tau --- band Frequency band for optical depth MHz N Running number of SNRs for remarks number=1 1. The highest absorption is observed in the direction of G0.0+0.0. According to [47], (a(5-1.4GHz)=0.7, and Sa(327MHz)=220Jy; from [48] Sobs(327MHz)=135Jy, that t(327MHz)=0.51, or, after reduction, t(100MHz)=6.14. 2. G0.9+0.1 is a classic example of a composite, two-component SNR including an extended (8') source with a steep (a=-0.64) spectrum and a central, more compact, component (2') with a flat spectrum (a=-0.1) [49]. The central component's contribution does not exceed 10% at 100MHz and S(1GHz) are shown for the extended component. 16. The higher absorption in the direction of G9.8+0.6 obtained in [7] is caused by the overestimated (a=-0.8) adopted by the author. 21. G12.0-0.1 is a two-component source with thermal and nonthermal components; according to Green [1] a=-1(?). 26. In the direction G16.8-1.1 thermal and nonthermal components were registered. The spectrum with the positive spectral index was observed at centimeter wavelengths [50]; the likely reason is thermal self-absorption. The table shows the spectral index of the nonthermal component. 58. Radio source G43.3-0.2 (W49B), has a possible spectrum break. The spectral index is a=0 at frequencies lower than 350MHz, and a=-0.47 at higher frequencies. 74. Radio source G69.0+2.7 (CTB 80) has an unusual spectrum. Possibly it has a break near 1GHz. In the frequency range f<=1GHz, a~=+0.3, and at f>=1GHz, a=-0.83. The compiled spectra of 9 SNRs: 4, 42, 52, 64, 73, 75, 99, 103, and 111, were not constructed. The spectral indices, without error, are taken from [1]. The absolute spectral index measurement accuracy of a>=0.15 was obtained for 26 SNRs: 2, 3, 10, 12, 15, 16, 17, 19, 44, 49, 59, 65, 66, 69, 72, 77, 80, 84, 88, 95, 98, 100, 101, 104, 107, and 110. Such great errors for 24% of the SNRs are the result of a large scatter of the compiled spectrum points, the low accuracy of the flux density measurements at different frequencies, and the small number of points. Several spectra, 98 and 110 for instance, were constructed using only two points: 83 and 408MHz. The smaller absolute measurement error, a>=0.1, had already been obtained for 70% of the SNRs. Absorption of SNR radio emission has yet to be observed for 42 SNRs (38%), see Table 2, column (11). The highest absorption was observed for four sources in the direction of the galactic central region: 1, 2, 3, and the unidentified source G0.4+0.1 [t(100MHz)=6-0.8]. In the direction of the other SNRs, the optical depth is t(100MHz)<=0.8. A high frequency (over 1 GHz) break in the spectrum was observed for seven SNRs: 30, 40, 77, 78, 84, 100, and 104. In all these cases, the spectrum was considerably steeper at frequencies above the break frequency than at the lower ones. The spectral index at high frequencies for these SNRs is given in the second row in the table. Spectra are drawn and discussed in [27]. New SNRs included in the catalog are: 3, 19, 68, and 99. SNRs with a flat spectrum (-a<=0.25) are: 7, 8, 10, 14, 31, 32, 38, 40, 58, 64, 73, and 111 - a total of 12 objects (11%). SNRs with a steep spectrum (-a>=0.7) are: 21, 22, 23, 27, 40, 74, 75, 77, 78, 79, 87, 100, and 104 a total of 13 objects (12%). SNRs with a high relative spectral index measurement accuracy (da/a<=0.1) are: 5, 18, 21, 23, 41, 45, and 53 a total of 7 objects (6%). -------------------------------------------------------------------------------- References: 1. Green, 1991PASP...13..209G 7. Kassim, 1989AJ...347..915K 11. Udal'tsov et al., 1978XI All-Union Radio Astronomy Conf.,Erevan...132U 27. Kovalenko et al., 1994AZh...71..92K 47. Ekkers et al., 1983A&A...122..143E 49. Helfand et al., 1989ApJ...341..151H 50. Furst et al., 1990A&AS...155..185F --- Veta Avedisova INASAN 1996 Sep 30 J_AZh_71_110.xml Spectral Investigation of NGC 7469 Using Image-Tube Observations from 1972-1990. J/AZh/71/200 J/AZh/71/200 Spectral Investigation of NGC 7469 Spectral Investigation of NGC 7469 Using Image-Tube Observations from 1972-1990. V T Doroshenko S G Sergeev K K Chuvaev Astron. Zh. 71 200 1994 1994AZh....71..200D Balmer lines Galaxies, spectra This investigation is mainly related to hydrogen lines in the spectrum of NGC 7469 from the 1972-1990 data obtained using an image tube on the 2.6-m telescope of the Crimean Astrophysical Observatory. The decomposition of the hydrogen lines into broad and narrow components was performed. Variations in the intensities and broad-component contours were observed. One third of the spectrograms showed a broad, symmetric Ha line, while the others showed asymmetry: the blue wings fall more steeply than the red ones. The degree of asymmetry is variable, but no correlation between it and the brightness of the nucleus was found. This asymmetry becomes weaker when passing to higher members of the Balmer series. The halfwidths of the broad components increase from Ha to H{gamma}. Redshifts of broad components with respect to narrow ones might also be larger for higher members of the Balmer series. Intensities of the broad hydrogen lines follow continuum variations with a delay of about 28 days. The Balmer decrement for broad lines is much flatter than for narrow ones.
NGC 7469 23 03 15.3 +08 52 25
Equivalent widths of the emission lines in NGC 7469 Date Observation date "DD/MM/YY" H(alpha)b Equivalent width of H(alpha) broad line 0.1nm H(alpha)n Equivalent width of H(alpha) narrow line 0.1nm [NII]6548 Equivalent width of [NII] 6548 A 0.1nm [NII]6583 Equivalent width of [NII] 6583 A 0.1nm H(beta)b Equivalent width of H(beta) broad line 0.1nm H(beta)n Equivalent width of H(beta) narrow line 0.1nm [OIII]4959 Equivalent width of [OIII] 4959 A 0.1nm [OIII]5007 Equivalent width of [OIII] 5007 A 0.1nm H(gamma)b Equivalent width of H(gamma) broad line 0.1nm H(gamma)n Equivalent width of H(gamma) narrow line 0.1nm Veta Avedisova INASAN 1996 Dec 30 J_AZh_71_200.xml Study of Two HgMn Stars with Suspected Anomalies of Noble Gas Abundances. J/AZh/71/588 J/AZh/71/588 Study of Two HgMn Stars Study of Two HgMn Stars with Suspected Anomalies of Noble Gas Abundances. L A Zakharova Astron. Zh. 71 588 1994 1994AZh....71..588Z Spectroscopy Stars, peculiar Three spectra of HD182308 (HR 7361) and four spectra of HD178065 (HR 7245) were obtained from 1989 to 1990 with the Main Stellar Spectrograph of the 6-m telescope at the Special Astrophysical Observatory and with the Coude spectrograph of the 2-m telescope of the Rozhen Observatory of the Bulgarian Academy of Sciences. Spectra were obtained in the range of 3700-4900A with inverse dispersion of 9 A/mm. Spectral resolution was close to 0.25A. Elemental abundances of two HgMn stars, HD 178065 and HD 182308, were found.
HD 182308 19 19 46.03 +64 23 26.7 HD 178065 19 07 08.95 +00 38 29.3
Parameters of lines Ion Ion --- Lambda Wavelength 0.1nm loggf Oscillator strength (log gf) --- r_loggf References for log gf number=1 References: 14. Kurucz & Peytremann, 1975, SAO Spec. Rep. 362, 2919. 16. Weise et al., 1966, NSRDS-NBS4, Washington: US Gov. Print.Office. 17. Weise & Martin, 1980, NSRDS-NBS68, part 1,Washington: US Gov. Print. Office. 18. Weise et al.,1969, NSRDS-NBS4, Washington: US Gov.Print. Office. 19. Artru et al., 1981A&AS...44..171A 20. Kurucz, 1992RMxAA..23...45K 21. Martin & Fuhr, 1975, J. Phys. Chem. Ref. Data 263, 218. 22. Younger et al., 1978, J. Phys. Chem. Ref. Data 7, 495. 23. Sigut & Landstreet, 1990MNRAS.247..611S 24. Smith, 1976MNRAS.177..275S 25. Jugaku et al., 1961ApJ...134..783J 26. Allen, 1976PASP...88..338A 27. Grevess et al., 1981, Upper MS CP Stars, 23rd Liege Ap. Coll., 211. 28. Grevess, 1984PhS.....8...49G --- W178065 Equivalent width (Angstroms) for HD178065 0.1nm W182308 Equivalent width (Angstroms) for HD182308 0.1nm n178065 line abundance log(N(I)/N(H)) for HD178065 --- n182308 line abundance log(N(I)/N(H)) for HD182308 --- Veta Avedisova INASAN 1997 Jan 28 J_AZh_71_588.xml UBVJHKLM Photometry of Nova Cygni 1992. J/AZh/71/618 J/AZh/71/618 UBVJHKLM Photometry of Nova Cygni 1992 UBVJHKLM Photometry of Nova Cygni 1992. E A Kolotilov A E Nadzhip V I Shenavrin B F Yudin Astron. Zh. 71 618 1994 1994AZh....71..618K Novae Photometry, UBVRIJKLMNH The results of photometric UBVJHKLM observations of Nova Cygni 1992 performed from the 83d until the 290th day after the nova outburst are presented. The accuracy of the brightness estimate was better than 0.03mag for UBVJHK, 0.05mag for L, and 0.1mag for M bands.
NOVA Cyg 1992 V1974 Cyg NOVA 1938 in M14 17 37 38.2 -03 14 42
Results of Nova Cygni 1992 photometric observations JD Date d Vmag V color mag B-V B-V color mag U-B U-B color mag Jmag J color (1.20um) mag Hmag H color (1.62um) mag Kmag K color (2.20um) mag Lmag L color (3.50um) mag Mmag M color (5.00um) mag Veta Avedisova INASAN 1997 Jan 20 J_AZh_71_618.xml Photometrically Distinct Nuclei in Elliptical and Early-Type Disk Galaxies. J/AZh/71/706 J/AZh/71/706 BV photometry of galactic nuclei Photometrically Distinct Nuclei in Elliptical and Early-Type Disk Galaxies. O K Silchenko Astron. Zh. 71 706 1994 1994AZh....71..706S Galaxies, photometry Morphology Using all data in the literature on multiaperture photometry in B and V bands for 237 galaxies, a list of candidates for galaxies with chemically distinct nuclei is compiled. Twenty-five to 50 percent of galaxies with morphological types from E to Sb are found to be such candidates.
Photometric characteristics of elliptical galaxies Name Name of the galaxy --- Note Notes number=1 Strong extinction in the galactic plane: NGC 2663 has A(B) = 1.33, NGC 3136 has A(B) = 1.94 (De Vaucouleurs et al. Second Reference Catalogue of Bright Galaxies, 1976, Cat. <VII/112>) --- Dist Distance Mpc u_Dist Uncertainty flag on Distance --- M(B) B absolute magnitude mag u_M(B) Uncertainty flag on B absolute magnitude --- Riarc Inner boundary radius of a studied region of a galaxy arcsec Rilin Inner boundary radius of a studied region of a galaxy kpc (B-V)Ri B-V color of the central part of a galaxy limited by inner radius mag Roarc Outer boundary of a studied region of a galaxy where there is no color gradient arcsec Rolin Outer boundary of a studied region of a galaxy where there is no color gradient kpc (B-V)Ro B-V color of a studied region of a galaxy mag e_(B-V)Ro Error on (B-V)Ro mag Grad Indicator of the presence of significant (B-V) color gradient --- Nucleus Degree of nucleus distinction number=2 1 - distinction on level 1 sigma, 2 - distinction on level 2 sigma, and so on. + indicate red nuclei, - indicate blue nuclei --- Photometric characteristics of bulges of lenticular galaxies Photometric characteristics of disks of lenticular galaxies Photometric characteristics of bulges of early-type spiral galaxies Photometric characteristics of disks of early-type spiral galaxies Name Name of the galaxy --- Dist Distance Mpc u_Dist Uncertainty flag on Distance --- M(B) B absolute magnitude mag u_M(B) Uncertainty flag on B absolute magnitude --- Riarc Inner boundary radius of a studied region of a galaxy arcsec Rilin Inner boundary radius of a studied region of a galaxy kpc (B-V)Ri B-V color of the central part of a galaxy limited by inner radius mag Roarc Outer boundary of a studied region of a galaxy where there is no color gradient arcsec Rolin Outer boundary of a studied region of a galaxy where there is no color gradient kpc (B-V)bul B-V color of a studied region of a galaxy number=1 Labels for table3 and table5 change to (B-V)disk mag e_(B-V)bul Error on (B-V)Ro number=2 Labels for table3 and table5 change to e_(B-V)disk mag Refs References number=3 References: B81 = Boroson, 1981ApJS...46..177B M92 = Magrelli Et al., 1992MNRAS.256..500M SV8 = Simien & de Vaucouleurs, 1986ApJ...302..564S K84 = Kent, 1984ApJS...56..105K K86 = Kent, 1986AJ.....91.1301K K88 = Kent, 1988AJ.....96..514K Gr = Grosbol, 1985A&AS...60..261G --- Grad Indicator of the presence of significant (B-V) color gradient --- Nucleus Degree of nucleus distinction number=4 1 = distinction on level 1 sigma, 2 = distinction on level 2 sigma, and so on. + indicate red nuclei, - indicate blue nuclei --- Veta Avedisova INASAN 1997 Jan 20 J_AZh_71_706.xml Polarimetric Observations of BL Lac J/AZh/71/717 J/AZh/71/717 Polarimetric Observations of BL Lac Polarimetric Observations of BL Lac V A Gagen-Torn S G Marchenko A V Yurchenko V A Yakovleva Astron. Zh. 71 717 1994 1994AZh....71..717G BL Lac objects Polarization This paper continues publications that report the results of photoelectric polarization measurements of the blazar BL Lac. Earlier, we published observational data obtained over the period 1969-1982 (Gagen-Torn et al., 1984AZh....61..925G). Here, we discuss the observations over the period 1983-1991.
BL Lac 22 02 43.3 +42 16 40
Results from polarimetric observations of BL Lac Date Date of observation (month, day) --- Year Year of the observation. yr JD Julian Day d P Polarization parameters P % u_P Uncertainty flag on P --- e_P Error on P % Q Polarization parameters Q deg u_Q Uncertainty flag on Q --- e_Q Error on Q deg d Flag for aperture used in the observation: 1 - 18.8" ; 3 - 26.7" --- Fo/Fb Ratio of the object flux to the background flux --- N Number of observations --- Veta Avedisova INASAN 1997 Jan 29 J_AZh_71_717.xml Spectroscopic Study of a Sample of Radio Sources from the 87GB Catalog J/AZh/72/12 J/AZh/72/12 Spectroscopy of Sources from 87GB Catalog Spectroscopic Study of a Sample of Radio Sources from the 87GB Catalog M Mingaliev A Khabrakhmanov Astron. Zh. 72 12 1995 1995AZh....72...12M VIII/14 : 87GB Catalog of radio sources (Gregory et al., 1991) VIII/42 : Texas Survey of radio sources at 365MHz (Douglas+ 1996) Radio sources A sample of 112 sources with flux densities higher than 200mJy at the 4.85GHz and with the range of declinations from +3 till +5 degrees from the Green Bank survey catalog 87GB <VIII/14> was observed at three frequencies: 0.96, 3.95, and 11.1GHz. The observations were performed in January and February 1992, in the Northern sector of the RATAN-600 radio telescope. The accuracy of the source right ascensions was improved by a factor of 5-10 (for 70% of the sources the accuracy of the right ascension is 0.1arcsec). About 80% of the objects studied were identified with sources from the Texas survey.
Radio spectra of a sample of 112 sources RAh Right ascension (1950) from 87GB h RAm Right ascension (1950) from 87GB min RAs Right ascension (1950) from 87GB s DE- Declination sign --- DEd Declination (1950) from 87GB deg DEm Declination (1950) from 87GB arcmin DEs Declination (1950) from 87GB arcsec RARh Right ascension (1950) (RATAN-600) h RARm Right ascension (1950) (RATAN-600) min RARs Right ascension (1950) (RATAN-600) s e_RARs Uncertainty in Right ascension (1950) s Flux2.7 Flux density in the 2.7cm (11.1GHz) Jy l_e_Flux2.7 Limit symbol on relative uncertainty of flux densities in the 2.7cm --- e_Flux2.7 Relative uncertainty of flux densities in the 2.7cm Jy l_Flux6.2 Limit symbol on flux density in the 6.2cm --- Flux6.2 Flux density in the 6.2cm (4,8GHz) Jy e_Flux6.2 Relative uncertainty of flux densities in the 6.2cm Jy Flux7.6 Flux density in the 7.6cm (3.9GHz) Jy e_Flux7.6 Relative uncertainty of flux densities in the 7.6cm Jy Flux31 Flux density in the 31cm (970MHz) Jy l_e_Flux31 Limit symbol on relative uncertainty of flux densities in the 31cm --- e_Flux31 Relative uncertainty of flux densities in the 31cm Jy Flux82 Flux density in the 82cm (370MHz) Jy e_Flux82 Relative uncertainty of flux densities in the 82cm Jy alpha1 Spectral index from 14P and 15P --- alpha2 Spectral index from 14P and 15P --- Rem Remarks # = The spectral indices were determined from flux densities at 7.6 and 31cm (in the absence of identification with the Texas survey) * = the source is from the Sternberg Astronomical Institute survey list ** = the source is identified with the adjacent lobe *** = the source signal was not distinguished because of interference from a nearby background source. The flux densities at 6.2 and 82cm from the Green Bank and Texas surveys. ref = a reference object --- Veta Avedisova INASAN 1997 May 10 J_AZh_72_12.xml A 95 GHz Survey of Methanol Masers J/AZh/72/22 J/AZh/72/22 A 95 GHz Survey of Methanol Masers A 95 GHz Survey of Methanol Masers I E Valtts A M Dzyura S V Kalenskii V I Slysh R Bus A Vinnberg Astron. Zh. 72 22 1995 1995AZh....72...22V J/AZh/71/37 : Thermal Methanol from 33 Clouds at 48 GHz (Slysh+ 1994) Interstellar medium Masers Radio lines A 95GHz survey of methanol emission in the 8_0_-7_1_A^+^ transition was conducted with the 20-m radio telescope at Onsala. Twenty-six new sources were detected in the emission line. At least nine out of the 35 studied sources are masers.
Gaussian parameters of spectral features in the sources emitting in the 95GHz methanol line Name Name of the source --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec F95 Flux of the line at 95 GHz Jy e_F95 Mean error on F95 Jy F Integrated flux Jy.km/s Vlsr Velocity km/s e_Vlsr Uncertainty in Vlsr km/s DV Line width km/s e_DV Uncertainty in DV km/s Veta Avedisova INASAN 1997 May 05 J_AZh_72_22.xml Variability at Frequencies 3.9 and 7.5 GHz: Radio Sources from the Zelenchukskii Survey with Fluxes > 200mJy. J/AZh/72/291 J/AZh/72/291 Variability at Frequencies 3.9 and 7.5 GHz Variability at Frequencies 3.9 and 7.5 GHz: Radio Sources from the Zelenchukskii Survey with Fluxes > 200mJy. A G Gorshkov V K Konnikova Astron. Zh. 72 291 1995 1995AZh....72..291G Radio sources A complete sample of radio sources from the Zelenchukskii survey with fluxes S(3.9GHz)>200mJy and declination range from +4 till +6 degrees were observed at 3.9 and 7.5GHz over the course of seven years. There are one hundred and eighty radio sources in the sample.
A complete sample of radio sources from the Zelenchukskii survey with fluxes S3.9>200mJy RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Note If * fluxes and spectral index were changed by authors in comparison printed version --- F3.9 Mean weighted fluxes at 3.9GHz (7.7cm) mJy F7.5 Mean weighted fluxes at 7.5GHz (4cm) mJy a Spectral index (3.9-7.5GHz) for the mean weighted fluxes. Spectral index was not calculated for extended sources. --- vF3.9 Relative variability amplitudes at 3.9GHz for sources with probability of variability greater than 0.95 --- vF7.5 Relative variability amplitudes at 7.5GHz for sources with probability of variability greater than 0.95 --- Pvar Probability of variability 1-(n-1) at 7.5GHz --- Ident Optical identification Q = known quasar SO= stellar object G = galaxy EF= empty field on the Palomar Sky Survey image L = Lacertae object F = object too faint for establishment of morphological type PR=populated region St= star --- Vmag Stellar magnitude mag z Redshift --- Ref References for the optical identifications --- Veta Avedisova INASAN 1997 May 10 J_AZh_72_291.xml Orientation of Circumstellar Disks and the Statistics of H{alpha} Profiles of Ae/Be Herbig Stars. J/AZh/73/194 J/AZh/73/194 Circumstellar Disks of Ae/Be Herbig Stars Orientation of Circumstellar Disks and the Statistics of H{alpha} Profiles of Ae/Be Herbig Stars. V P Grinin A N Rostopchina Astron. Zh. 73 194 1996 1996AZh....73..194G Polarization Stars, early-type Stars, emission Orion stars Ae/Be stars circumstellar matter The data of the photo-polarimetric activity of Ae/Be Herbig stars and the types of Ha profiles observed in their spectra was carried out using data from the literature. The analysis of the data supports the presence of a relationship between the type of Ha profile and the level of photo-polarimetric activity in young stars.
Photometric activity and the profiles of H{alpha} lines of Ae/Be Herbig stars No Running number --- Star Name of star number=1 polarisation and brightness are presented for the V band except for the star HR 5999 (flagged by 'B' in n_Vmin) which are in B band. --- SpType Spectral type --- Vmin Faintest magnitude for the V band number=1 polarisation and brightness are presented for the V band except for the star HR 5999 (flagged by 'B' in n_Vmin) which are in B band. mag Vmax Brightest magnitude for the V band number=1 polarisation and brightness are presented for the V band except for the star HR 5999 (flagged by 'B' in n_Vmin) which are in B band. mag n_Vmin Vmin and Vmax refer to B band number=1 polarisation and brightness are presented for the V band except for the star HR 5999 (flagged by 'B' in n_Vmin) which are in B band. --- Halpha Types of H-alpha profile accodingly to Finkenzeller and Mundt (1984A&AS...55..109F) --- Ref1 References for the photometry (list below) --- Pmin Minimal degree of polarization number=1 polarisation and brightness are presented for the V band except for the star HR 5999 (flagged by 'B' in n_Vmin) which are in B band. % n_Pmin Pmin refers to right polarization --- Pmax Maximum degree of polarization number=1 polarisation and brightness are presented for the V band except for the star HR 5999 (flagged by 'B' in n_Vmin) which are in B band. % n_Pmax Pmax refers to right polarization --- Vamp Amplitude of variations during polarization measurements number=1 polarisation and brightness are presented for the V band except for the star HR 5999 (flagged by 'B' in n_Vmin) which are in B band. mag Ref2 References to polarization data --- Veta Avedisova INASAN 1996 Sep 30 J_AZh_73_194.xml The energy distribution in the visible spectrum for the 27 giants and supergiants of the M spectral type J/AZh/73/762 J/AZh/73/762 Energy distribution in giants and supergiants. The energy distribution in the visible spectrum for the 27 giants and supergiants of the M spectral type V M Tereshchenko Astron. Zh. 73 762 1996 1996AZh....73..762T Energy distributions Stars, giant giants supergiants energy distributions The energy distributions for 27 giants and supergiants of the M spectral type are presented in the region of 3200-7600{AA} with the step of 50{AA}. The observations were made in the Fessenkov Astrophysical institute (Alma-Ata) during 1986-1987 with a spectrophotometer of Seya-Namioka mounted on the 50-cm Cassegrain telescope. The primary standard is Vega with the energy distribution by Hayes (1985IAUS..111..225H). The relative r.m.s. of the results are given in the table3.dat.
Stars positions HD HD (Cat. <III/135>) name --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Energy distribution lambda Spectral line wavelength 0.1nm HD36389 Energy distribution for HD 36389 10-8W/m2/cm HD42543 Energy distribution for HD 42543 10-8W/m2/cm HD44537 Energy distribution for HD 44537 10-8W/m2/cm HD78712 Energy distribution for HD 78712 10-8W/m2/cm HD206936 Energy distribution for HD 206936 10-8W/m2/cm HD1760 Energy distribution for HD 1760 10-8W/m2/cm HD19058 Energy distribution for HD 19058 10-8W/m2/cm HD20797 Energy distribution for HD 20797 10-8W/m2/cm HD23475 Energy distribution for HD 23475 10-8W/m2/cm HD197812 Energy distribution for HD 197812 10-8W/m2/cm HD224062 Energy distribution for HD 224062 10-8W/m2/cm HD18191 Energy distribution for HD 18191 10-8W/m2/cm HD18345 Energy distribution for HD 18345 10-8W/m2/cm HD55383 Energy distribution for HD 55383 10-8W/m2/cm HD55966 Energy distribution for HD 55966 10-8W/m2/cm HD56031 Energy distribution for HD 56031 10-8W/m2/cm HD69243 Energy distribution for HD 69243 10-8W/m2/cm HD77443 Energy distribution for HD 77443 10-8W/m2/cm HD80390 Energy distribution for HD 80390 10-8W/m2/cm HD84748 Energy distribution for HD 84748 10-8W/m2/cm HD123657 Energy distribution for HD 123657 10-8W/m2/cm HD132813 Energy distribution for HD 132813 10-8W/m2/cm HD184786 Energy distribution for HD 184786 10-8W/m2/cm HD196610 Energy distribution for HD 196610 10-8W/m2/cm HD202012 Energy distribution for HD 202012 10-8W/m2/cm HD222800 Energy distribution for HD 222800 10-8W/m2/cm HD224490 Energy distribution for HD 224490 10-8W/m2/cm Information about the stars Seq Running number --- HR Bright Star (Cat. <V/50>) number --- HD Henry Draper (Cat. <III/135>) number --- Names Other Names --- Vmag V magnitude mag B-V B-V color index mag U-B U-B color index mag Sptype Spectral type --- VarType Type of variability --- The observations and the accuracy of the results HD Henry Draper (Cat. <III/135>) number --- Dates Observation dates --- Std Standard star names --- Nobs Number of observations --- dM The difference of air masses dM is the difference of air masses of the program star and the standard star. --- dt The difference of time dt is the difference of time of the observations of the program star and the standard star min sigma1 rms in the range 3200-4000{AA} % sigma2 rms in the range 4000-5000{AA} % sigma3 rms in the range 5000-6000{AA} % sigma4 rms in the range 6000-7600{AA} % Veta Avedisova INASAN 1997 Mar 17 J_AZh_73_762.xml Spectra of weak radio sources from the RATAN-600 "Kholod" deep survey J/AZh/74/42 J/AZh/74/42 RATAN-600 radio sources spectra Spectra of weak radio sources from the RATAN-600 "Kholod" deep survey N N Bursov Astron. Zh. 74 42 1997 1997AZh....74...42B VIII/33 : Spectral characteristics of RATAN (RC) Catalog (Bursov+ 1989) J/A+AS/87/1 : RATAN-600 7.6 cm radio sources catalog (Parijskij+ 1991) J/other/BSAO/40.128 : RATAN-600 radio sources spectra (Bursov 1996) J/other/BSAO/40.5 : RATAN-600 RC radio sources (Parijskij+ 1996) Radio sources Spectroscopy A multifrequency deep survey of a band of sky with the declination of the source SS 433 ({delta}~5{deg}+/-20') was performed as part of the "Kholod" program on the RATAN-600 in 1987-1988. The right ascension intervals covered by the survey are 0h<{alpha}<14h and 18h<{alpha}<24h. The spectral properties of 400 sources from the RC catalog were determined for the first time by using only RATAN-600 data. The maximum in the flux density distribution for these sources at the central wavelength, {lambda}7.6cm, occurs at ~30mJy. The lower flux limits for the sample at wavelengths of 3.9, 7.6, 13.0, and 31.0cm are 16, 9, 37, and 61mJy, respectively. These observations provide the first flux estimates at 13.0 and 31.0cm for 90% of the sources. Spectra were measured for the first time for 112 sources (28%) and were revised for 90 sources (23%). The maximum in the spectral index distribution for the entire sample in the interval from {lambda}{lambda}7.6-31.0cm occurs at {alpha}=-0.86+/-0.04 (S_v_~{nu}^{alpha}^). The spectra of some 20 of the sample sources (5%) are peaked at roughly 1GHz, and about 40 spectra (10%) have low-frequency breaks. Roughly 70 sources (19%) have flat spectra ({alpha}>-0.5), and 64 (18%) have very steep spectra ({alpha}<-1.1).
Flux densities for RC radio sources (1988.0) Seq Sequential number --- RC Name of the source in the RC catalogue derived from the coordinates for the epoch J2000 --- n_RC Corrected or new spectrum number=1 n: sources with the spectra obtained for the first time c: sources with revised or corrected spectra For the rest of the sources, spectra was added --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Shift Shift in height {DELTA}h from the centre of the antenna beam arcmin l_S3.9cm Limit flag on S3.9cm --- S3.9cm Flux density at {lambda}3.9cm (7GHz) mJy n_S3.9cm n: Flux values is lacking --- e_S3.9cm rms uncertainty on S3.9cm mJy l_S7.6cm Limit flag on S7.6cm (3.9GHz) --- S7.6cm Flux density at {lambda}7.6cm mJy n_S7.6cm n: Flux values is lacking --- e_S7.6cm rms uncertainty on S7.6cm mJy l_S13.0cm Limit flag on S13.0cm --- S13.0cm Flux density at {lambda}13.0cm (2.3GHz) mJy n_S13.0cm n: Flux values is lacking --- e_S13.0cm rms uncertainty on S13.0cm mJy l_S31.0cm Limit flag on S31.0cm --- S31.0cm Flux density at {lambda}31.0cm (0.96GHz) mJy n_S31.0cm n: Flux values is lacking --- e_S31.0cm rms uncertainty on S31.0cm mJy SI Calculated spectral index from {lambda}{lambda}7.6-31.0cm --- Spectrum Type of the source spectrum number=2 Types from the classification of Kellerman (1974, in, Galactic and Extragalactic Radio Astronomy, ed: G.L. Verschuur and K.I. Kellerman, Springer-Verlag, berlin, Heildelberg, New-York, 320.). S: linear power-law spectra associated with extended optically thin radio sources. C-: The spectrum has a negative second derivative of the dependence logS-log{nu} and is more steep at the short wavelengths. Such spectra are also assigned to extended radio sources Cmax: The power spectrum (class S) or dual power spectrum (class C-) at short waves, but there is a sharp cut off at the long wavelengths. Such spectra are produced by compact optically thick sources. C+: The spectrum has positive curvature with a rise at the long or the short wavelengths. CPX: Complex spectra with one or more minima. The spectra are generally believed to be composed of two or more spectra of class Cmax plus, in some case, of class S. The spectra of this class are also assigned to compact optically thick objects. F: Flat spectra --- James Marcout, Patricia Bauer CDS 1998 Nov 16 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_AZh_74_42.xml Analysis of compact radio sources using 102 MHz interplanetary scintillation observations J/AZh/74/812 J/AZh/74/812 102MHz radio source survey Analysis of compact radio sources using 102 MHz interplanetary scintillation observations S A Tyul'bashev Astron. Zh. 74 812 1997 1997AZh....74..812T Radio lines Radio sources An analysis of 125 radio sources from a 102MHz survey of scintillating sources is presented. These compact (<1") radio sources are identified with radio sources in the most sensitive catalogs currently available. Analysis of the integrated spectra for these objects indicates that the compact sources have steep spectra ({alpha}>0.5). There is a tendency for weaker sources to be more compact. The inferred spectral indices for compact sources in the cores of extended objects are on average lower than the integrated values. The most likely candidates for optical counterparts to the compact radio sources from the scintillating source survey are steep-spectrum quasars.
Source flux densities, spectral indices, and compactnesses Name Source name (based on 1950 position) --- rms rms fluctuation for the scintillating source flux density at 102MHz Jy S102MHz Flux density at 102MHz Jy S151MHz Integrated flux density at 151MHz Jy S365MHz Integrated flux density at 365MHz Jy S408MHz Integrated flux density at 408MHz Jy S1400MHz Integrated flux density at 1400MHz Jy S4885MHz Integrated flux density at 4885MHz Jy SI Spectral index for the integrated spectra --- l_R Limit flag on R --- R Compactness of the source number=1 Ratio of the flux density of the scintillating component to the integrated flux density of the source. --- u_R Uncertainty flag on R --- James Marcout, Patricia Bauer CDS 1998 Nov 13 UNKNOWN UNKNOWN Prepared via OCR at CDS. * 01-Mar-1999: three errors were detected in the English version (1997ARep...41..723T) by H. Andernach: -> 1 source (0612+396) is missing -> missing l_R flag for 0636+397 -> bad name (1649+485) for 0649+485 J_AZh_74_812.xml The 5C5 survey of radio sources. J/MNRAS/171/475 J/MNRAS/171/475 The 5C5 survey of radio sources. The 5C5 survey of radio sources. T J Pearson Mon. Not. R. Astron. Soc. 171 475 1975 1975MNRAS.171..475P J/MNRAS/182/273 : 5C6 and 5C7 Survey of Radio Sources J/MNRAS/200/747 : 5C12 Survey of Radio Sources Kellermann, K.I, Pauliny-Toth, I.I.K. & Davies, M.M. 1968, Astrophys. Lett., 2, 105. Radio continuum Radio sources Surveys This catalog contains the 5C5 survey of radio sources, one of a series of deep surveys made at 408 MHz (HPBW 80"x109") and 1407 MHz (HPBW 23"x31") with the One-Mile telescope at Cambridge. The 5C5 survey was centered on 09h40m+47d (B1950) and contains 252 sources stronger than 8.7 mJy at 408 MHz and 1.8 mJy at 1407 MHz. The flux densities are on the KPW scale (Kellermann et al. 1969ApJ...157....1K), and were based on 3C48. This table was originally published in Pearson, T.J (1975MNRAS.171..475P)
5C5 Survey of Radio Sources (RA: 9.5h-9.9h; DEC: 44.5{deg} -49.5{deg} ) Name Name of source number=1 The serial number of the 5C5 source is given in this column. The sources in each survey are numbered in increasing order of right ascension. Occasionally two sources are grouped together in the lists, and given suffixes a, b; this is done either when there are two peaks of emission at 1407 MHz but only one at 408 MHz, or when there is an obvious association between the two sources. The IAU nomenclature has not been adopted because this position-based system would be ambiguous for some of the 5C sources which are very close together. The authors recommend that when it is necessary to refer to a source by its 5C name in a context in which its position is not obvious, the 5C name should be accompanied by the IAU name in parentheses, thus: 5C5.103 (0938+467). --- RAh Right Ascension (B1950) (hour) number=2 These columns give the B1950.0 right ascension and declination of the radio source. Positions measured at 1407 MHz are flagged with an asterisk ('*') in the ext_flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission, the positional error (pos_err) is listed as blank and 'ext_flag' is marked 'e'. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=2 These columns give the B1950.0 right ascension and declination of the radio source. Positions measured at 1407 MHz are flagged with an asterisk ('*') in the ext_flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission, the positional error (pos_err) is listed as blank and 'ext_flag' is marked 'e'. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec pos_err Positional uncertainty in R.A. number=2 These columns give the B1950.0 right ascension and declination of the radio source. Positions measured at 1407 MHz are flagged with an asterisk ('*') in the ext_flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission, the positional error (pos_err) is listed as blank and 'ext_flag' is marked 'e'. arcsec ext_flag Flagged 'e' if extended number=2 These columns give the B1950.0 right ascension and declination of the radio source. Positions measured at 1407 MHz are flagged with an asterisk ('*') in the ext_flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission, the positional error (pos_err) is listed as blank and 'ext_flag' is marked 'e'. --- S408 408 MHz flux density number=3 These columns give flux density information at 408 MHz. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to- noise ratio). An asterisk in the f_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1) These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy e_S408 Error on 408 flux density number=3 These columns give flux density information at 408 MHz. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to- noise ratio). An asterisk in the f_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1) These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy f_S408 '*' flux density is almost certainly wrong number=3 These columns give flux density information at 408 MHz. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to- noise ratio). An asterisk in the f_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1) These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- att_408 Envelope attenuation at 408 MHz number=3 These columns give flux density information at 408 MHz. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to- noise ratio). An asterisk in the f_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1) These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- S1407 Flux density at 1407 MHz number=4 These columns give flux density information at 1407 MHz. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15) These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy e_S1407 Error on 1407 flux density number=4 These columns give flux density information at 1407 MHz. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15) These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy f_S1407 '*' flux density is almost certainly wrong number=4 These columns give flux density information at 1407 MHz. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15) These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- att_1407 Envelope attenuation at 1407 MHz number=4 These columns give flux density information at 1407 MHz. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15) These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- Sp-Index Spectral index between 408 and 1407 MHz number=5 This column gives the spectral index between 408 and 1407 MHz. Alpha is defined in the sense S {prop.to} {nu}^-{alpha}^. --- comments Comments on the source number=6 This column gives comments on the source. The following abbreviations are used: ARG Half-Mile telescope Survey at 1421 MHz (Gillespie, 1975MNRAS.170..541G) KPD 5 GHz KPD survey (Kellermann et al. 1968) --- Patricio Ortiz CDS 1999 Apr 06 UNKNOWN UNKNOWN "The catalogue was originally archived as A068 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_MNRAS_171_475.xml The 5C6 and 5C7 surveys of radio sources. J/MNRAS/182/273 J/MNRAS/182/273 The 5C6 and 5C7 surveys of radio sources. The 5C6 and 5C7 surveys of radio sources. T J Pearson Mon. Not. R. Astron. Soc. 182 273 1978 1978MNRAS.182..273P J/MNRAS/171/475 : The 5C5 survey of radio sources J/MNRAS/200/747 : 5C12 Survey of Radio Sources Pilkington, J.D.H., and Scott, P.F. 1965, Mem.R.A.S., 69, 183. Ryle, M. 1972, Nature, 239, 435. Radio continuum Radio sources Surveys This catalog contains the 5C6 and 5C7 radio surveys at 408 and 1407 MHz done with the with the One-Mile telescope at Cambridge (UK). The 5C6 survey of radio sources, made at 408 MHz (HPBW 80"x151") and 1407 MHz (HPBW 23"x44") was centered on 02:14 +32:00' (B1950) and contains 297 sources stronger than 10 mJy at 408 MHz and 1.5 mJy at 1407 MHz. The flux densities are on the KPW scale (Kellermann et al. 1969ApJ...157....1K) and were based on 3C147 and 3C380. Positions, positional errors, flux density information, and descriptions of optical objects visible on the Palomar Sky Survey within about 20" of the radio sources are given. The 5C7 survey of radio sources, made at 408 MHz (HPBW 80"x176") and 1407 MHz (HPBW 23"x51") was centered at 08:17 +27:00 (B1950) and contains 281 sources stronger than 10 mJy at 408 MHz and 1.5 mJy at 1407 MHz. The flux densities are on the KPW scale (Kellermann et al. 1969ApJ...157....1K), and were based on 3C147 and 3C380. Positions, positional errors, flux density information, and descriptions of optical objects visible on the Palomar Sky Survey within about 20" of the radio sources are given.
5C6 Survey of Radio Sources (RA: 2h - 2.4h; DEC: 29.5{deg} - 34.3{deg}) 5C6 Name of source number=1 The serial number of the 5C6 source is given in this column. The sources in each survey are numbered in increasing order of right ascension. Occasionally two sources are grouped together in the lists, and given suffixes a, b; this is done either when there are two peaks of emission at 1407 MHz but only one at 408 MHz, or when there is an obvious association between the two sources. The IAU nomenclature has not been adopted because this position-based system would be ambiguous for some of the 5C sources which are very close together. The authors recommend that when it is necessary to refer to a source by its 5C name in a context in which its position is not obvious, the 5C name should be accompanied by the IAU name in parentheses, thus: 5C6.103 (0212+297). --- RAh Right Ascension (B1950) (hour) number=3 These columns give the B1950.0 right ascension and declination of the radio source, Positions measured at 1407 MHz are flagged with an asterisk ('*') in the Pos_Flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission and the positional error (ext_flag) is listed as 'e'. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=3 These columns give the B1950.0 right ascension and declination of the radio source, Positions measured at 1407 MHz are flagged with an asterisk ('*') in the Pos_Flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission and the positional error (ext_flag) is listed as 'e'. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Pos_Flag '*' if position is from 21 cm observation number=3 These columns give the B1950.0 right ascension and declination of the radio source, Positions measured at 1407 MHz are flagged with an asterisk ('*') in the Pos_Flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission and the positional error (ext_flag) is listed as 'e'. --- e_RAs Positional uncertainty in RA number=4 This column gives the RA positional uncertainty, in arcsec, excluding any systematic error. The uncertainties in declination are greater by cosec dec (cosec({delta})). An 'e' in column 'ext_flag' means that the source is extended and the position given is the peak of emission. Uncertainties vary depending on the intensity and frequency of the observation. arcsec ext_flag Extension flag number=4 This column gives the RA positional uncertainty, in arcsec, excluding any systematic error. The uncertainties in declination are greater by cosec dec (cosec({delta})). An 'e' in column 'ext_flag' means that the source is extended and the position given is the peak of emission. Uncertainties vary depending on the intensity and frequency of the observation. --- l_S408 Flagged if flux density is uncertain or upper limit number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit or an '(' if the flux density is estimated. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk "*" in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- S408 408 MHz flux density number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit or an '(' if the flux density is estimated. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk "*" in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy e_S408 Error on 408 flux density number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit or an '(' if the flux density is estimated. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk "*" in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy f_e_S408 flux density error flag number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit or an '(' if the flux density is estimated. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk "*" in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- att_408 Envelope attenuation at 408 MHz number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit or an '(' if the flux density is estimated. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes a contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk "*" in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- f_S1407 Flagged if 1407 flux density could not be determined number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- S1407 Flux density at 1407 MHz number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy e_S1407 Error on 1407 flux density number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy f_e_S1407 flux density error flag number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- att_1407 Envelope attenuation at 1407 MHz number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- l_Sp-Index [<] Flagged if alpha is an upper limit number=6 These columns give the spectral index flag and spectral index between 408 and 1407 MHz. The alpha_flg column is marked with a '<' if alpha is an upper limit. Alpha is defined in the sense S {prop.to} {nu}^-{alpha}^. --- Sp-Index Spectral index between 408 and 1407 MHz number=6 These columns give the spectral index flag and spectral index between 408 and 1407 MHz. The alpha_flg column is marked with a '<' if alpha is an upper limit. Alpha is defined in the sense S {prop.to} {nu}^-{alpha}^. --- comments Comments on the source number=7 This column gives comments on the source, including descriptions of optical objects within 15-20 arcsec. The parameter 'r' is given for sources detected at 1407 MHz on both high- and low-resolution maps; r = * means that r could not be determined accurately. The following abbreviations are used: conf confused sl slightly pa position angle N North S South f following p preceeding m magnitude The references to other observations are as follows: 3C Third Cambridge Catalogue (3C 200 only) (Cat.<VIII/1>) 4C Fourth Cambridge Catalogue (Pilkington and Scott 1965) (Cat.<VIII/4>) AO Arecibo Occultation Survey (Hazard, Gulkis, and Sutton 1968ApJ...154..413H) B2 Bologna Survey (Colla et al. 1970A&AS....1..281C, 1972A&AS....7....1C, 1973A&AS...11..291C) Cat.<VIII/36> GC NRAO 5-GHz Survey (Davis 1971AJ.....76..980D) MW One-Mile Telescope fan-beam Survey (Willson 1972MNRAS.156....7W) PKS Parkes Survey (Shimmins and Day 1968AuJPh..21..377S) W Westerbork 1415 MHz Survey (Willis, Oosterbaan and de Ruiter 1976A&AS...25..453W) 5-km Observations with the Cambridge 5-km telescope (HPBW 2") (Ryle 1972) --- 5C7 Survey of Radio Sources (RA: 8.1h - 8.4h; DEC: 24.3{deg} - 29.6{deg}) 5C7 Name of source number=1 The serial number of the 5C7 source is given in this column. The sources in each survey are numbered in increasing order of right ascension. Occasionally two sources are grouped together in the lists, and given suffixes a, b; this is done either when there are two peaks of emission at 1407 MHz but only one at 408 MHz, or when there is an obvious association between the two sources. The IAU nomenclature has not been adopted because this position-based system would be ambiguous for some of the 5C sources which are very close together. The authors recommend that when it is necessary to refer to a source by its 5C name in a context in which its position is not obvious, the 5C name should be accompanied by the IAU name in parentheses, thus: 5C7.103 (0815+266). --- RAh Right Ascension (B1950) (hour) number=3 These columns give the B1950.0 right ascension and declination of the radio source, Positions measured at 1407 MHz are flagged with an asterisk ('*') in the Pos_Flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission and the positional error (ext_flag) is listed as 'e'. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=3 These columns give the B1950.0 right ascension and declination of the radio source, Positions measured at 1407 MHz are flagged with an asterisk ('*') in the Pos_Flag column and are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). For extended sources, the position given is the peak of emission and the positional error (ext_flag) is listed as 'e'. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Pos_Flag '*' if position is from 21cm obs. number=4 This column gives the RA positional uncertainty, in arcsec, excluding any systematic error. The uncertainties in declination are greater by cosec dec (cosec({delta})). An 'e' in column 'ext_flag' means that the source is extended and the position given is the peak of emission. Uncertainties vary depending on the intensity and frequency of the observation. --- e_RAs Positional uncertainty in RA number=4 This column gives the RA positional uncertainty, in arcsec, excluding any systematic error. The uncertainties in declination are greater by cosec dec (cosec({delta})). An 'e' in column 'ext_flag' means that the source is extended and the position given is the peak of emission. Uncertainties vary depending on the intensity and frequency of the observation. arcsec ext_flag extension flag 'e' if extended number=4 This column gives the RA positional uncertainty, in arcsec, excluding any systematic error. The uncertainties in declination are greater by cosec dec (cosec({delta})). An 'e' in column 'ext_flag' means that the source is extended and the position given is the peak of emission. Uncertainties vary depending on the intensity and frequency of the observation. --- l_S408 '<' if flux density is an upper limit number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S1407 column, which includes contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- S408 408 MHz flux density number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S1407 column, which includes contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy e_S408 Error on 408 flux density number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S1407 column, which includes contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy f_e_S408 Flag on error estimation number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S1407 column, which includes contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- att_408 Envelope attenuation at 408 MHz number=2 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S1407 column, which includes contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). An asterisk in the f_e_S408 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.1). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- f_S1407 Flagged if 1407 flux density could not be determined number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- S1407 Flux density at 1407 MHz number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy e_S1407 Error on 1407 flux density number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. mJy f_e_S1407 Flag on error estimation number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- att_1407 Envelope attenuation at 1407 MHz number=5 These columns give flux density information at 1407 MHz. The f_S1407 column is '+' if the position was measured at 1407 MHz but the flux density could not be determined. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. An asterisk in the f_e_S1407 column indicates that the uncertainty in flux density is very large because the source lies outside the measured part of the envelope (attenuation factor less than 0.15). These sources are included in the table only for their positions; many of them have been observed in other surveys so it is possible to check the positional accuracy. --- f_Sp-Index Flagged if alpha is an upper limit number=6 These columns give the spectral index flag and spectral index between 408 and 1407 MHz. The alpha_flg column is marked with a '<' if alpha is an upper limit. Alpha is defined in the sense S {prop.to} {nu}^-{alpha}^. --- Sp-Index Spectral index between 408 and 1407 MHz number=6 These columns give the spectral index flag and spectral index between 408 and 1407 MHz. The alpha_flg column is marked with a '<' if alpha is an upper limit. Alpha is defined in the sense S {prop.to} {nu}^-{alpha}^. --- comm Comments on the source number=7 This column gives comments on the source, including descriptions of optical objects within 15-20 arcsec. The parameter 'r' is given for sources detected at 1407 MHz on both high- and low-resolution maps; r = * means that r could not be determined accurately. The following abbreviations are used: conf confused sl slightly pa position angle N North S South f following p preceeding m magnitude The references to other observations are as follows: 3C Third Cambridge Catalogue (3C 200 only) (Cat.<VIII/1>) 4C Fourth Cambridge Catalogue (Pilkington and Scott 1965) (Cat.<VIII/4>) AO Arecibo Occultation Survey (Hazard, Gulkis, and Sutton 1968ApJ...154..413H) B2 Bologna Survey (Colla et al. 1970A&AS....1..281C, 1972A&AS....7....1C, 1973A&AS...11..291C) Cat.<VIII/36> GC NRAO 5-GHz Survey (Davis 1971AJ.....76..980D) MW One-Mile Telescope fan-beam Survey (Willson 1972MNRAS.156....7W) PKS Parkes Survey (Shimmins and Day 1968AuJPh..21..377S) W Westerbork 1415 MHz Survey (Willis, Oosterbaan and de Ruiter 1976A&AS...25..453W) 5-km Observations with the Cambridge 5-km telescope (HPBW 2") (Ryle 1972) --- Patricio Ortiz CDS 1999 Apr 06 UNKNOWN UNKNOWN "The catalogue was originally archived as A020 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_MNRAS_182_273.xml A deep radio/optical survey near the North Galactic Pole. I. The 5C12 catalogue. J/MNRAS/200/747 J/MNRAS/200/747 5C12: survey near the North Galactic Pole A deep radio/optical survey near the North Galactic Pole. I. The 5C12 catalogue. C R Benn G Grueff M Vigotti J V Wall Mon. Not. R. Astron. Soc. 200 747 1982 1982MNRAS.200..747B J/MNRAS/171/475 : The 5C5 survey of radio sources J/MNRAS/182/273 : 5C6 and 5C7 Survey of Radio Sources Pilkington, J.D.H. and Scott, P.F. 1965, Mem.R.A.S., 69, 183. Williams, P.J.S., Kenderdine, S., and Baldwin, J.E. 1966, Mem.R.A.S., 70, 53. Galactic pole, north Radio continuum Radio sources Surveys This catalog contains a deep survey (5C12) of a region close to the North Galactic Pole carried out with the Cambridge One-Mile Telescope at 408 MHz (HPBW 80"x139") and at 1407 MHz (HPBW 23"x40"). The flux densities are on the KPW scale (Kellermann et al. 1969ApJ...157....1K), and were based on 3C48, 3C147 and 3C295. This part of the survey contains 321 sources with apparent flux densities brighter than 9 mJy at 408 MHz or 1.4 mJy at 1407 MHz.
5C12 Survey of Radio Sources (RA: 12.75h-13.2h; DEC: 32.7{deg} - 38.3{deg}) 5C12 Name of source number=1 The serial number of the 5C12 source is given in this column. The sources in each survey are numbered in increasing order of right ascension. Occasionally two sources are grouped together in the lists, and given suffixes a, b; this is done either when there are two peaks of emission at 1407 MHz but only one at 408 MHz, or when there is an obvious association between the two sources. The IAU nomenclature has not been adopted because this position-based system would be ambiguous for some of the 5C sources which are very close together. The authors recommend that when it is necessary to refer to a source by its 5C name in a context in which its position is not obvious, the 5C name should be accompanied by the IAU name in parentheses, thus: 5C12.103 (1256+328). --- RAh Right Ascension (B1950) (hour) number=2 These columns give the B1950.0 right ascension and declination of the radio source. Positions measured at 1407 MHz are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=2 These columns give the B1950.0 right ascension and declination of the radio source. Positions measured at 1407 MHz are accurate to an extra decimal place in right ascension and declination (2 decimal places in RA and 1 in declination). --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec e_RAs RA positional uncertainty number=3 These columns give the positional uncertainty in right ascension and declination, in arcsec. If there is evidence for resolution of the source (see notes column below), the errors given here are underestimates. arcsec e_DEs Dec positional uncertainty number=3 These columns give the positional uncertainty in right ascension and declination, in arcsec. If there is evidence for resolution of the source (see notes column below), the errors given here are underestimates. arcsec l_S408 '<' if flux density is an upper limit number=4 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). --- S408 408 MHz flux density number=4 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). mJy e_S408 Error on 408 flux densit (4)y mJy att_408 Envelope attenuation at 408 MHz number=4 These columns give flux density information at 408 MHz. The l_S408 column contains a '<' if the flux density is an upper limit. The flux density is given in the S408 column. The rms uncertainty in the 408 MHz flux density is given in the e_S408 column, which includes contribution of 3 percent uncertainty in the envelope correction. The att_408 column gives the envelope attenuation factor at 408 MHz (multiply S by this factor to recover S' and hence the signal-to-noise ratio). --- S1407 Flux density at 1407 MHz number=5 These columns give flux density information at 1407 MHz. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. mJy e_S1407 Error on 1407 flux density number=5 These columns give flux density information at 1407 MHz. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. mJy att_1407 Envelope attenuation at 1407 MHz number=5 These columns give flux density information at 1407 MHz. The flux density is given in the S1407 column. The rms uncertainty in the 1407 MHz flux density is given in the e_S1407 column, and the att_1407 column gives the envelope attenuation factor at 1407 MHz. --- l_Sp-Index Flagged if alpha is an upper limit number=6 These columns give the spectral index flag and spectral index between 408 and 1407 MHz. The l_alpha column is marked with a '<' if alpha is an upper limit. Alpha is defined in the sense S {prop.to} {nu}^-{alpha}^. For sources undetected at the higher frequency in 5C12, 1415 MHz flux densities from Katgert et al. (1973A&A....23..171K) have been used. --- Sp-Index Spectral index between 408 and 1407 MHz number=6 These columns give the spectral index flag and spectral index between 408 and 1407 MHz. The l_alpha column is marked with a '<' if alpha is an upper limit. Alpha is defined in the sense S {prop.to} {nu}^-{alpha}^. For sources undetected at the higher frequency in 5C12, 1415 MHz flux densities from Katgert et al. (1973A&A....23..171K) have been used. --- obslist List of observations number=7 This column gives a list of other detections. The following abbreviations are used: Survey MHz Limit Beam Reference (mJy) --------------------------------------------------------------------------- WKB 38 14000 45' Williams, Kenderdine, and Baldwin (1966) 4C 178 200 15'x8' Pilkington and Scott (1965) (Cat.<VIII/4>) A0 318 500 16' Veron and Veron (1979A&AS...36..331V) WK 408 70 3'x10' Windram and Kenderdine (1969MNRAS.146..265W) GV 408 200 3'x10' Grueff and Vigotti (1968ApL.....2..113G) B2.1 408 200 3'x10' Colla et al. (1970A&AS....1..281C) B2.3 408 250 3'x10' Colla et al. (1973A&AS...11..291C) W6 610 12 53"x92" Katgert (1978A&AS...31..409K) W 1415 7 23"x40" Katgert et al. (1973A&A....23..171K) OH 1420 160 10'x40' Dixon and Kraus (1968AJ.....73..381D) DA 1420 1000 36' Galt and Kennedy (1968AJ.....73..135G) K2 2700 2 4"x6" 5-km telescope K5 5000 2 2"x4" 5-km telescope GC 5000 49 3' Davis (1971AJ.....76..980D) --- struct Structural information on the source number=8 This column gives structural information on the source. The following abbreviations are used: dbl double p possibly resolved r information from ratio between 1407 MHz flux densities measured from low- and high-resolution maps u unresolved v information from visibility measured as a function of baseline Other codes in parentheses indicate the source of the information according to the abbreviation in the obslist column above. 4 = 408 MHz (5C12); 14 = 1407 MHz (5C12). --- notes Notes on the source number=9 This column gives notes on the source. An asterisk indicates that further information on the source is given in the notes appended to the table in the original paper. --- Patricio Ortiz CDS 1999 Apr 06 UNKNOWN UNKNOWN "The catalogue was originally archived as A021 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_MNRAS_200_747.xml A Neutral Hydrogen Survey of the Southern Galactic Plane for |b|< 10 deg. J/MNRAS/201/495 J/MNRAS/201/495 HI Survey of Southern Galactic Plane A Neutral Hydrogen Survey of the Southern Galactic Plane for |b|< 10 deg. A W Strong P A Riley J L Osborne Mon. Not. R. Astron. Soc. 201 495 1982 1982MNRAS.201..495S H I data Interstellar matter Radio sources Surveys A survey of atomic hydrogen 21-cm line emission in the Galactic plane, covering the region 12 deg > l > 245 deg and |b| < 10 degrees. The survey was performed in 1981 using the Parkes 64-m telescope and sky sampling intervals of 0.5 degrees in galactic longitude and 1 degree in galactic latitude. The observed range in V(LSR) is between +/-211 km/s, with a velocity resolution of 0.824 km/s. The rms noise of the observations is quoted as ~1 K, and effects of stray radiation on the observations are stated to be smaller than errors in the temperature scale calibration. This survey was designed to supplement the northern hemisphere HI survey of Weaver and Williams (1973). Taken together, the two surveys provided complete (though undersampled) 21-cm observations of the sky within +/- 10 deg of the Galactic plane. Note, however, that a later survey by Kerr et al. (1986) provided a fully-sampled southern dataset with higher sensitivity than that of Strong et al. The survey data are archived as a single FITS file. The FITS image is stored as a data cube, with LSR velocity on the first axis, galactic latitude on the second axis, and galactic longitude as the third. The 21-cm line intensity is quoted as a brightness temperature.
strong82.fit HI data cube for southern Galactic plane J. Weiland ADF/ADC 1998 Oct 07 Thanks to H. Andernach [U. Guanajuato, Mexico] for locating the data file. J_MNRAS_201_495.xml Bright extragalactic radio sources at 2.7 GHz- III. The all-sky catalogue. J/MNRAS/216/173 J/MNRAS/216/173 Bright extragalactic radio sources at 2.7 GHz Bright extragalactic radio sources at 2.7 GHz- III. The all-sky catalogue. J V Wall J A Peacock Mon. Not. R. Astron. Soc. 216 173 1985 1985MNRAS.216..173W BL Lac objects Galaxies, radio QSOs Radio continuum Radio sources The brightest extragalactic radio sources at 2.7 GHz are catalogued. The complete sample comprises 233 sources found in the major centimeter wavelength surveys carried out at ANRAO/Parkes, NNRAO/Greenbank, and MPIfR/Bonn: the sample covers 9.81 sr and has limits S(27) = 2.0 Jy and |b| > 10{deg}. A critical reanalysis of the data shows that 227 (97 percent) have optical identifications and 171 (73 percent) have measured redshifts. The implications of the catalogue statistics for the luminosity functions of different radio-source populations are considered.
All Sky Catalog of Extragal. Radio Srcs at 2.7 GHz IAUname Name of source in IAU convention number=1 The 'IAUname' column gives the name of the source in IAU convention. The 'Name' column gives an alternative name, if available. --- Name Other name of source number=1 The 'IAUname' column gives the name of the source in IAU convention. The 'Name' column gives an alternative name, if available. --- RAh Right Ascension (B1950) (hour) number=2 These columns give the B1950 right ascension and declination of the source. Positions are from the first reference listed in the "r_RAh" column, and are optical positions with the following exceptions: if the optical position was of low accuracy and the source was compact, the radio position was used. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=2 These columns give the B1950 right ascension and declination of the source. Positions are from the first reference listed in the "r_RAh" column, and are optical positions with the following exceptions: if the optical position was of low accuracy and the source was compact, the radio position was used. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec poserr Positional error of source number=3 This column gives the positional error. The quoted error is the rms in one direction in arcsec. arcsec S11cm Flux density at 11cm (2.7 GHz) number=4 This column gives the flux density at 2.7 GHz, in Jy. The 2.7 GHz flux-density scale was changed from that used by Kellermann et al. (1969ApJ...157....1K) to the Parkes flux-density scale. Jy Sp-Index Spectral index of source between 2.7 & 5 GHz number=5 This column gives the spectral index between 2.7 and 5 GHz, in the sense of S {prop.to} {nu}^-{alpha}^. --- Otype Optical identification type number=6 This column gives the optical classification of the source, as follows: Q QSO confirmed by spectrum or variability (and including BL Lac objects). Q? Stellar object on position. G Galaxy confirmed by extended image. G? Very faint object; presumed galaxy. EF Empty field --- Vmag V magnitude of source mag z Redshift of source number=7 These columns give the redshift and redshift flag. The f_z column is marked with an asterisk ('*') if the redshift is an estimate. --- f_z Flag '*' if z is estimated number=7 These columns give the redshift and redshift flag. The f_z column is marked with an asterisk ('*') if the redshift is an estimate. --- r_RAh Reference for position number=8 References to the given position are as follows: A '???' indicates that the entries in that column are not complete. The author intends to go back and fill in the missing info in the future. --- References code reference code --- reftxt Bibcode (if any) and reference text --- Patricio Ortiz CDS 1999 Apr 06 UNKNOWN UNKNOWN Prepared from the tables available at the "ADS Catalogue Service" (CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA) J_MNRAS_216_173.xml The dynamics of rich clusters - I. Velocity data J/MNRAS/224/453 J/MNRAS/224/453 Velocity data of rich clusters The dynamics of rich clusters - I. Velocity data M Colless P Hewett Mon. Not. R. Astron. Soc. 224 453 1987 1987MNRAS.224..453C Clusters, galaxy Redshifts Velocity dispersion We present redshifts and stellar velocity dispersions for about 40 galaxies in each of 14 rich clusters from the southern cluster survey of Abell & Corwin (1983, Early Evolution of the Universe and Its Present Structure, p.179, Eds. Abell & Chincarini, Reidel, Dordrecht, Holland). The clusters cover a wide range of richnesses and Abell and Bautz-Morgan types, our aim being to compile a large, homogeneous database for examining and comparing dynamical phenomena and morphological properties. Further papers will present photometry for the clusters and an analysis of the database.
C02 ACO 2717 00 03.3 -35 57 C03 ACO 2721 00 06.1 -34 43 C19 ACO 3126 03 28.7 -55 43 C20 DRCG 0329-52 03 30.2 -52 34 C21 ACO 458 03 45.8 -24 18 AC1 Str 0409-597 04 09.5 -59 35 C30 ACO 3334 05 18.0 -58 33 C31 ACO 3360 05 40.3 -43 24 C37 ACO 3705 20 41.7 -35 14 C39 ACO S 906 20 42.3 -51 57 C52 ACO 3854 22 17.7 -35 43 C64 ACO 2538 23 08.7 -19 53 C65 ACO 2554 23 12.3 -21 29 C67 Braid 272 23 52.1 -34 23
Velocity sample for the clusters Cluster Cluster name --- Gal Galaxy identifier --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec cz Heliocentric radial velocity km/s e_cz rms uncertainty on cz km/s sigma Stellar velocity dispersion km/s e_sigma rms uncertainty on sigma km/s R Reliability measure number=1 R: ratio of peak height to noise in the cross-correlation function, which is used to calculate the errors and is a measure of the combined effects of noise and template mismatch (see Tonry & Davis, 1979AJ.....84.1511T). --- Note Notes number=2 Method by which velocities were obtained: Blank: cross-correlation E: emission lines A: absorption features E+A: emission and absorption features --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Jun 19 UNKNOWN UNKNOWN Prepared via OCR at CDS. * 02-Oct-1997: Four errors detected by H. Andernach were corrected in table3 J_MNRAS_224_453.xml CCD photometry of galactic clusters containing Cepheid variables - IV. NGC 6649 J/MNRAS/224/61 J/MNRAS/224/61 NGC 6649 UBV photometry CCD photometry of galactic clusters containing Cepheid variables - IV. NGC 6649 A R Walker C D Laney Mon. Not. R. Astron. Soc. 224 61 1987 1987MNRAS.224...61W Clusters, open Photometry, CCD Stars, variable A colour magnitude diagram to V=20 is given for 395 stars in the heavily reddened open cluster NGC 6649. The absorption-corrected distance modulus is 11.00+/-0.15mag (1585+/-110pc) assuming R(OB)=3.27+/-0.10 for NGC 6649 and based on a ZAMS with zero point referenced to a Pleiades distance modulus of 5.56mag. The range of reddening over the 5arcmin diameter of the cluster is {DELTA}E(B-V)=0.3mag. NGC 6649 contains the double mode Cepheid V367 Sct, which has <M_V_>=-3.80+/-0.06 and <B_0_>-<V_0_>=0.58+/-0.02.
NGC 6649 18 33.5 -10 24
Photometry of NGC 6649 stars No Sequential number --- DRA Offest in right ascension number=1 Coordinates with respect to star No. 19, in the sense that any star to the NE of star No. 19 has positive DRA and DDE. arcsec DDE Offest in declination number=1 Coordinates with respect to star No. 19, in the sense that any star to the NE of star No. 19 has positive DRA and DDE. arcsec Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag o_Vmag Number of observation in V magnitude --- o_Bmag Number of observation in B magnitude --- o_Umag Number of observation in U magnitude --- Marie-Jose Wagner, Patricia Bauer CDS 1997 Jun 19 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_224_61.xml The Cambridge IPS Survey at 81.5 MHz J/MNRAS/229/589 J/MNRAS/229/589 Interplanetary Scintillation Survey at 81.5 MHz The Cambridge IPS Survey at 81.5 MHz A Purvis S J Tappin W G Rees A Hewish P J Duffett-Smith Mon. Not. R. Astron. Soc. 229 589 1987 1987MNRAS.229..589P Radio sources Pulsars Galaxies, radio QSOs A catalog of 1789 radio sources which exhibit interplanetary scintillation (IPS) at 81.5 MHz is presented. The angular diameters of scintillating components in the range 0.2-2 arcsec are listed together with values of the scintillating flux density at a solar elongation of 90 deg. IPS selects those sources which are highly compact, such as pulsars and some unusual extragalactic sources, or those in which energy is being released from active beams in the outer lobes of intrinsically powerful radio galaxies and quasars. The survey was made with the 3.6-hectare array at Cambridge and covers the area of sky between declinations -10 deg and +83 deg at all values of right ascension. The array was operated as a north-south phase-switching interferometer observing sources near meridian transit. Sixteen declination beams were produced covering the observed declination range. The half-power width of a declination beam is 5.5 sec(52.16-DEC) degrees, where DEC is the declination of peak beam response. The half-power beam width in right ascension is 107 sec(delta) s for a source at declination delta. The faintest sources in the catalogue have scintillating flux densities of about 0.3 Jy rms at a solar elongation of 90 deg, and total flux densities of about 5 Jy at 81.5 MHz. The sensitivity of the survey is not uniform over the sky, being determined largely by the galactic background emission. The flux density corresponding to one source per beam area in this survey is about 2.3 Jy at 81.5 MHz so that confusion errors are likely to be significant for total flux density S <= 20 Jy.
List of 1789 scintillating radio sources Name Source Name --- RAh Right Ascension (1950) h RAm Right Ascension (1950) min RAs Right Ascension (1950) number=1 Correct within +/- 5 s of time. s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin n_DEd Note on declination number=2 I: determined by computer algorithm, typical error 30 arcmin. H: determined by hand, typical error 30 arcmin. C: source is confused, central declination of the beam is listed, error ~1/2 of declination beamwidth. N: insufficient data to determine declination, central declination of the beam is listed, error ~1 declination beamwidth. B: adjacent beam record apparently contradictory, central declination of the beam is listed, error ~1/2 of declination beamwidth. --- dS_90 Scintillating flux density at solar elongation of 90 degrees number=3 The median scintillating flux density in the elongation range 80-100 degrees. Scintillating flux density is the rms variation of total flux density. Jy Diam Angular diameter number=4 Derived by fitting theoretical curves from the model of Readhead et al. (1978MNRAS.185..207R) to the data between elongations 40 and 90 degrees. arcsec Dmin One sigma error limit on Diam arcsec Dmax One sigma error limit on Diam arcsec n_Diam Note on Diam number=5 +: Estimate of Diam is not reliable because data is sparse. S: Very sparse data, Diam value not given. P: Pulsar like curve, Diam value not given. H: High ecliptic latitude source, Diam value not given. --- Sc Compact flux density for scintillating component number=4 Derived by fitting theoretical curves from the model of Readhead et al. (1978MNRAS.185..207R) to the data between elongations 40 and 90 degrees. Jy Sc_min One sigma error limit on Sc Jy Sc_max One sigma error limit on Sc Jy Ident Possible contributing sources number=6 The antenna pattern was too broad for reliable identifications in most cases, so several possible contributing sources may be listed. ^1 following a source name indicates it makes only a minor contribution to the measured signal. ^2 indicates confusion by a system artefact. * indicates a 4C source for which positional agreement would be improved by lobe shifting. --- N. Odegard SSDOO/ADC 1999 Nov 01 UNKNOWN UNKNOWN An electronic version of the data table was obtained from http://www.mrao.cam.ac.uk/surveys/ips/index.html . H. Andernach informed ADC of minor differences between the MRAO web version and the published version of the data table. The version here is in agreement with the published version. J_MNRAS_229_589.xml An optical spectrophotometric survey of abundances in Magellanic Cloud planetary nebulae J/MNRAS/234/583 J/MNRAS/234/583 Abundances in Magellanic Cloud planetary nebulae An optical spectrophotometric survey of abundances in Magellanic Cloud planetary nebulae D J Monk M J Barlow R E S Clegg Mon. Not. R. Astron. Soc. 234 583 1988 1988MNRAS.234..583M J/ApJS/75/407 : PNe Magellanic Cloud optical spectroscopy. I J/ApJS/76/1085 : PNe Magellanic Cloud optical spectroscopy. II J/ApJS/83/87 : PNe Magellanic Cloud optical spectroscopy. III J/A+AS/121/407 : LMC planetary nebulae positions (Leisy+ 1997) Magellanic Clouds Nebulae, planetary Spectroscopy Optical spectroscopic data for 71 Planetary Nebulae (PN) in the Large and Small Magellanic Clouds have been analysed. The line fluxes have been used to determine nebular temperatures, densities, and the abundances of He, N, O, Ne and Ar, relative to H. In our sample there are 12 nebulae with N/O>=0.5, resembling Peimbert's Type I PN; six low-excitation objects [1<=I(5007)/I(H{beat})<=4], and four very-low excitation (VLE) nebulae [I(H{beta})>I(5007)], similar to the Galactic VLE class. Mean abundances have been calculated for the nebulae not in these special groups. After correction for collisional excitation contributions to the nebular He I lines, PN in the SMC and LMC yield mass fractions of Y=0.249+/-0.025 and Y=0.258+/-0.012, respectively.
Corrected relative line intensities for LMC PN: medium resolution Corrected relative line intensities for LMC PN: low resolution Corrected relative line intensities for SMC PN: medium resolution Corrected relative line intensities for SMC PN: low resolution Lambda Wavelength 0.1nm ID Identification of the line --- PN Planetary nebula identification --- Name Planetary nebula name --- l_I(Lambda) limit flag on I(Lambda) --- I(Lambda) Measured line intensity (I(Hbeta)=100) --- u_I(Lambda) Uncertainty flag on I(Lambda) --- Patricia Bauer CDS 1996 Oct 03 Pierre Leisy <leisy@iap.fr> J_MNRAS_234_583.xml A survey for metrewave variability extragalactic radio sources. J/MNRAS/235/1313 J/MNRAS/235/1313 Metric wave Extragalactic Variability A survey for metrewave variability extragalactic radio sources. O B Slee B C Siegman Mon. Not. R. Astron. Soc. 235 1313 1988 1988MNRAS.235.1313S VIII/35 : Radio Sources observed with Culgoora Circular Array Slee O.B. 1995, Aust. J. Phys., 48, 143 =1995AuJPh..48..143S Slee O.B. 1994, Einstein On-line Service, 'rad_cul80_160' Slee O.B. et al. 1982, Proc. Astron. Soc. Aust. 4, 278 Slee O.B. et al. 1983, Proc. Astron. Soc. Aust., 5, 114 =1983PASAu...5..114S Slee O.B. and Siegman, B.C. 1988, MNRAS, 235, 1313 =1988MNRAS.235.1313S Radio sources We report a detailed statistical study of the intensity variations in 412 extragalactic radio sources randomly selected from the ~2000 sources which have been observed with the Culgoora circular array at 80 and 160 MHz during the interval 1970-84. Our results are: (i) About 47 per cent of the sample displays significant variability on time scales of months or years. (ii) A similar degree of variability is shown by QSOs, radio galaxies and sources in blank optical fields. (iii) Sources with flatter radio spectra are more variable. (iv) There is a weak increase in variability for the lower-galactic-latitude sources. (v) There is a correlation between month-to-month variability and year-to year variability in the same sources. (vi) The degree of variability at 80MHz is related to that at 160MHz. (vii) Most of the sources in both the variable and non-variable categories have a component with angular diameter <1arcsec. Our results are partly consistent with an origin in refractive scintillation by large-scale electron density turbulence in the intervening medium. There are, however, serious difficulties in explaining, from the existing theory of slow galactic scintillation, the short time-scale of the scintillation. Our results are probably more in accord with the focusing and occulting effects of compact interstellar ionized structures recently identified at microwave frequencies.
Variability Measurements from the Culgoora Circular Array Name Source name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec OptID Optical Identification --- z Redshift of optical identification --- alpha Radio spectral index --- GLON Galactic longitude deg GLAT Galactic latitude deg F80MHz Average flux density at 80 MHz Jy o_F80MHz Number of observations at F80MHz --- M1a 1-monthly 80 MHz modulation index number=1 Variability modulation indices as defined by Slee and Siegman (1988MNRAS.235.1313S). A value of '-1.00' means that no variability (95% confidence level) was detected. A blank indicates that the data were not available to test for variability. --- M12a 12-month 80 MHz modulation index number=1 Variability modulation indices as defined by Slee and Siegman (1988MNRAS.235.1313S). A value of '-1.00' means that no variability (95% confidence level) was detected. A blank indicates that the data were not available to test for variability. --- F160MHz Average flux density at 160 MHz Jy o_F160MHz Number of observations at F160MHz --- M1b 1-month 160 MHz modulation index number=1 Variability modulation indices as defined by Slee and Siegman (1988MNRAS.235.1313S). A value of '-1.00' means that no variability (95% confidence level) was detected. A blank indicates that the data were not available to test for variability. --- M12b 12-month 160 MHz modulation index number=1 Variability modulation indices as defined by Slee and Siegman (1988MNRAS.235.1313S). A value of '-1.00' means that no variability (95% confidence level) was detected. A blank indicates that the data were not available to test for variability. --- Patricia Bauer CDS 1996 Aug 21 We thank Heinz Andernach <hja@vilspa.esa.es> for providing an access to his set of radio catalogues (R190), and to Bruce Slee <BSLEE@rp.CSIRO.au> for his assistance. J_MNRAS_235_1313.xml An extended galaxy redshift survey - I. The catalogue J/MNRAS/236/207 J/MNRAS/236/207 Galaxy redshift catalogue An extended galaxy redshift survey - I. The catalogue N Metcalfe R Fong T Shanks D Kilkenny Mon. Not. R. Astron. Soc. 236 207 1989 1989MNRAS.236..207M VII/142 : Southern Redshifts (Fairall+ 1991) VII/193 : The CfA Redshift Catalogue (Huchra+ 1995) Galaxy catalogs Redshifts We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.
Catalogue n_Name Note on the galaxy number=1 * Indicates galaxy with superimposed star. ? This object has a stellar spectrum but is clearly diffuse on the plate. --- Name Galaxy name --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Bj Bj magnitude mag cz Heliocentric velocity (precision +/-130km/s) km/s r Largest r factor found from the cross-relation (where appropriate) number=2 only one of the two numbers, r or Nem, is provided. r is the ratio of the height of the true peak to the average peak in a(x). For more details, see Tonry & Davies (1979AJ.....84.1511T). --- Nem Number of emission lines used for velocity number=2 only one of the two numbers, r or Nem, is provided. r is the ratio of the height of the true peak to the average peak in a(x). For more details, see Tonry & Davies (1979AJ.....84.1511T). --- Date Observation date "MM/YY" Code See note number=3 0: emission line velocity 1,2 and 3: cross-correlation quality ratings in section 4.2 4: no redshift could be obtained from the spectrum 5: the one object whose redshift we took from RC2 Cat. <VII/112> 6: galaxies which have velocities, but are not in the one-third sampling criterion 9: two-thirds whose redshifts we did not attempt to measure --- Com Comments number=4 Any alternative designation for the objects (e.g. NGC number) is given here. Also, emission-line redshifts are given for those objects which showed emission but whose cross-correlation velocities were adopted for the survey. note E: Emission line velocities for objects whose cross-correlation velocities were deemed more reliable. The number of emission lines on which the measure is based is given in brackets. --- Marie-Jose Wagner, Patricia Bauer CDS 1996 Oct 25 It is a pleasure to thank Heinz Andernach who communicated the results of his own cross-checking and suggested an enhanced presentation of the data file. UNKNOWN UNKNOWN * March 1996: Prepared via OCR at CDS. * November 1996: Cross-checked versus printed table and corrected, J_MNRAS_236_207.xml The Parkes selected regions : deep optical and infrared observations of radio galaxies and quasars at high redshifts. J/MNRAS/238/1171 J/MNRAS/238/1171 Optical/IR observ. of Radio Galaxies and QSOs The Parkes selected regions : deep optical and infrared observations of radio galaxies and quasars at high redshifts. J S Dunlop J A Peacock A Savage S J Lilly J N Heasley A J B Simon Mon. Not. R. Astron. Soc. 238 1171 1989 1989MNRAS.238.1171D VIII/15 : Parkes Radio Sources Catalogue (PKSCAT90) Galaxies, radio Photometry, infrared Photometry, UBVRI QSOs This catalog reports on an extensive optical and infrared study of the 178 radio sources in the Parkes Selected Regions (S > 100 mJy at 2.7 GHz). CCD observations have resulted in the essential completion (95 percent) of optical identifications and have provided B and R photometry. In addition, K photometry has been completed for four of the six selected regions.
Optical and IR Study of Parkes Radio Sources (-22{deg} < Dec < 4{deg} ) Name IAU name of source number=1 This column gives the IAU name of the source, as given in the Parkes catalog (Cat.<VIII/15>). The source name is followed by an asterisk if the first interferometer observation of the sources was made by Downes et al. (1986MNRAS.218...31D). Sources which were revealed by the observations of Downes et al. to consist of several distinct sources have been labeled A, B, ... in order of increasing right ascension. Note that for sources 0223+018 and 1154-019 two optical counterparts are given, for which the radio data are simply repeated. This leads to a total of 180 rows for the 178 sources in this table. --- RAh Right Ascension (B1950) (hour) number=2 These columns give the B1950 right ascension and declination of the expected position for the optical identification. For unresolved or partly resolved sources this is the position of the radio peak. For doubles with central components the position of the central component has been used, while for doubles without central components the (unweighted) midpoint of the outer components is given. In D2 sources (see the struct column) the flat-spectrum component has been used. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) --- DEd Declination (B1950) (deg) number=2 These columns give the B1950 right ascension and declination of the expected position for the optical identification. For unresolved or partly resolved sources this is the position of the radio peak. For doubles with central components the position of the central component has been used, while for doubles without central components the (unweighted) midpoint of the outer components is given. In D2 sources (see the struct column) the flat-spectrum component has been used. deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec S2.7G Flux density at 2.7 GHz number=3 The 2.7 GHz flux density from the original survey is given in the "S2.7G" column (in Jy). The "f_S2.7G" column is marked with a colon (':') if the corresponding flux density was corrected by Downes et al. (1986MNRAS.218...31D) to allow for confusion. Jy f_S2.7G ':' if fluxes corrected for confusion --- Sp-Index Spectral index between 5 and 1.4 GHz number=4 The radio spectral index between 1.4 and 5 GHz is given in the "alpha" column. The "f_alpha" column is marked with a colon (':') if the spectral index is uncertain. Alpha is defined in the sense of S {prop.to} {nu}^-{alpha}^. --- u_Sp-Index ':' if spectral index is uncertain --- Struct Brief description of radio structure number=5 This column gives a brief description of the radio structure. The following abbreviations are used: U Unresolved. The flux density decreases by less than 10% on the longest baselines (d~25 km). P Partially resolved. The flux density decreases by more than 10% on the longest baselines, but no details of the structure are available. Do Double. CC Central component. Di Diffuse emission. V Variable. (1) indicates that variability was detected by Condon, Balonek, and Jauncey (1976AJ.....81..913C). D2 Flat-spectrum core and extended emission on one side only. H Diffuse halo. HT Head-tail structure. I/II Classification of the structure according to the scheme by Fanaroff and Riley (1974MNRAS.167P..31F) in which type II sources have hot spots separated by more than half the length of the source, while type I sources do not. --- ra_opt Last column of optical right asc. (B1950) number=6 These columns give the B1950 position of the optical identification. The positions are only given in the last unit (sec in right ascension and arcsec in declination). The larger units can be recovered from the radio source position. s dec_opt Last column of optical declination (B1950) number=6 These columns give the B1950 position of the optical identification. The positions are only given in the last unit (sec in right ascension and arcsec in declination). The larger units can be recovered from the radio source position. arcsec delta Offset between radio and optical positions number=7 This column gives the offset between the radio and optical positions, in arcsec. arcsec ID Optical classification number=8 This columns gives the optical identification as follows: Q Quasi-stellar, confirmed by spectroscopy, variability or colour (see the paper and Downes et al. 1986MNRAS.218...31D for details). Q? Stellar object on position, with colour classification suggesting it is probably a quasar. G Galaxy confirmed by image or colour. G? Faint object, possibly extended with colour classification suggesting it is probably a galaxy. EF Empty field. ? Uncertain optical classification. --- l_Bmag '>' if B magnitude is a lower limit --- Bmag Apparent B magnitude mag e_Bmag Uncertainty on B magnitude mag l_Rmag '>' if R magnitude is a lower limit --- Rmag Apparent R magnitude mag f_Rmag '?' if R magnitude is uncertain --- e_Rmag Uncertainty on R magnitude mag l_Kmag '>' if K magnitude is a lower limit number=9 These columns give the apparent K magnitude and associated uncertainty. l_Kmag is flagged with a greater-than symbol if the Kmag magnitude is a lower limit. f_Kmag is flagged with a '?' if the K magnitude is uncertain. f_Kmag is flagged with a '*' if the source was observed by Downes et al., 1986MNRAS.218...31D. --- Kmag Apparent K magnitude number=9 These columns give the apparent K magnitude and associated uncertainty. l_Kmag is flagged with a greater-than symbol if the Kmag magnitude is a lower limit. f_Kmag is flagged with a '?' if the K magnitude is uncertain. f_Kmag is flagged with a '*' if the source was observed by Downes et al., 1986MNRAS.218...31D. mag f_Kmag if Kmag is uncertain or from Downes number=9 These columns give the apparent K magnitude and associated uncertainty. l_Kmag is flagged with a greater-than symbol if the Kmag magnitude is a lower limit. f_Kmag is flagged with a '?' if the K magnitude is uncertain. f_Kmag is flagged with a '*' if the source was observed by Downes et al., 1986MNRAS.218...31D. --- e_Kmag Uncertainty on K magnitude number=9 These columns give the apparent K magnitude and associated uncertainty. l_Kmag is flagged with a greater-than symbol if the Kmag magnitude is a lower limit. f_Kmag is flagged with a '?' if the K magnitude is uncertain. f_Kmag is flagged with a '*' if the source was observed by Downes et al., 1986MNRAS.218...31D. mag z Redshift --- u_z Flagged '?' if redshift is uncertain --- r_ID Source references number=10 This column gives the references for (respectively) the optical position (C denotes COSMOS measurement by Downes et al.), the identification, the finding chart and the redshift; references qre sepqrqted by commas. --- References code reference code --- reftxt Bibcode (if available) and reference text --- Patricio Ortiz CDS 1999 Apr 07 UNKNOWN UNKNOWN "The catalogue was originally archived as A050 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_MNRAS_238_1171.xml Distance errors and the stellar luminosity function J/MNRAS/238/709 J/MNRAS/238/709 NPG stars VIJHK photometry Distance errors and the stellar luminosity function R S Stobie K Ishida J A Peacock Mon. Not. R. Astron. Soc. 238 709 1989 1989MNRAS.238..709S Photometry Stars, distances A study of the stellar luminosity function in the region of the north galactic pole (NPG) is described. The method is based on photometric parallaxes derived from the V-I colour index. A complete sample of stars is defined with I<16, V>13, V-I>1.5 and within 130pc of the Sun. JHK photometry is obtained for stars with V-I>2.9 to check the V-I calibration and exclude contamination by giants. It is demonstrated that application of the classical Malmquist bias derives an incorrect luminosity function. A detailed discussion is given of the effects of Malmquist-type biases on luminosity functions and a method presented which effectively deconvolves the observed luminosity function to determine the intrinsic luminosity function. The method is applied to the data in the north galactic pole sample. The derived main sequence luminosity function is in good agreement with other determinations based on the method of photometric parallaxes, showing a clear peak at M_v_~+11.5 to +12 and a well-defined decrease thereafter to M_v_=+15. Fainter than M_v_=+15, the luminosity function is not defined by the present study.
List of North Galactic Pole (NGP) stars within 130 pc of the Sun RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd DEclination (1950) deg DEm DEclination (1950) arcmin DEs DEclination (1950) arcsec Vmag V magnitude mag Imag I magnitude mag V-I V-I colour index mag Kmag K magnitude mag J-K J-K colour index mag H-K H-K colour index mag Marie-Jose Wagner, Patricia Bauer CDS 1997 Apr 29 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_238_709.xml Multicolour photometry of the cluster of galaxies Sersic 129-01 J/MNRAS/240/785 J/MNRAS/240/785 Multicolour photometry of Sersic 129-01 Multicolour photometry of the cluster of galaxies Sersic 129-01 S J C Millington J V Peach Mon. Not. R. Astron. Soc. 240 785 1989 1989MNRAS.240..785M Galaxies, photometry Redshifts Spectra, ultraviolet We describe photometry of 907 galaxies brighter than b26.25=20.5 in a 1.83X1.83 area centred on the southern cluster Sersic 129-01 in the u, b, r and i bands. The slopes and zero-points of the colour-absolute magnitude diagrams agree well with other clusters including Coma and the rich cluster Shapley 8 suggesting they are independent of cluster environment. The (u-b) against (b-i) diagram distinguishes well between morphological types. The reddening we obtain by a number of methods disagrees with that of Griersmith (1982). The L-sig relation has a similar form to other clusters and when combined with data for Virgo leads to a relative distance modulus which agrees with that from Griersmith's comparison of colour-magnitude diagrams only on the assumption of E (B-V) = 0.15 in front of the cluster and a high value of Ho. A mass of 7.4X10 13 Mo is found for the elliptical dominated component of the cluster and (M/L)b=59.
ubri photometry No Identification number --- Type '?' for probable galaxies, ';' when magnitudes could not be measured due to contamination by stars --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination 1950 (sign) --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Remark 'D' for double, 'E' for est.mag. --- Overlap '*' for overlapped image --- b26.25 b26.25 isophotoal magnitude mag R(b26.25) Effective radius at 26.25 mag/arcsec^2 limiting isophote arcsec b-r (b-r) equal area colour mag R(b-r) Radius of equal area colour arcsec u-b (u-b) equal area colour mag R(u-b) Radius of equal area colour arcsec b-i (b-i) equal area colour mag R(b-i) Radius of equal area colour arcsec Francois Ochsenbein CDS 1993 Jan 05 J_MNRAS_240_785.xml A catalogue of faint, UV-excess objects. J/MNRAS/243/1 J/MNRAS/243/1 A catalogue of faint UV-excess objects A catalogue of faint, UV-excess objects. B J Boyle R Fong T Shanks B A Peterson Mon. Not. R. Astron. Soc. 243 1 1990 1990MNRAS.243....1B J/MNRAS/251/482 : A spectroscopic survey of faint QSOs (Boyle+ 1991) Photometry, ultraviolet QSOsSpectra, ultraviolet Spectra, positions, magnitudes and colours are presented for 1400 faint (B<~21mag) stellar objects identified in a complete, ultraviolet-excess (UVX) survey. The objects were selected from COSMOS machine measurements of UK Schmidt U and J plates and observed with the Fibre Optic Coupled Aperture Plate (FOCAP) system at the Anglo-Australian Telescope (AAT). In total, 420 QSOs were identified, of which nine belong to the broad absorption line (BAL) class of QSOs. A further 57 galaxies with narrow emission lines were found. Halo subdwarfs from the vast majority (~90 per cent) of the 824 galactic stars identified in this survey; the remaining galactic stars are comprised principally of hot white dwarfs (42 objects) and horizontal branch stars (nine objects). Updated versions of the QSO number-magnitude relation and luminosity function derived from this survey are also presented in this paper.
The QSO catalogue The stellar catalogue Unidentified Objects Name Extended IAU coordinate designation --- FOCAP_ID FOCAP area name followed by the fibre number --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec b Calibrated COSMOS magnitude mag u-b Colour obtained from calibrated COSMOS magnitude mag ID Identification of object number=1 QSO = Qso with broad emission lines, QSO? = possible QSO, BLAQ = broad absorption line QSO, NL = narrow emission line object, CONT = object with continuum spectrum. Comp = composite --- z emission line redshift --- q_z Estimate of the redshift quality number=2 Redshift quality: 1: certain redshift 2: probable redshift; e.g. usually obtained from one strong line and additional low signal-to-noise lines visible 3: uncertain redshift; e.g. only one strong line or only low signal-to-noise lines visible --- Lyalpha Rest equivalent width of the emission lines of Lyalpha + N V --- CIV Rest equivalent width of the emission lines of CIV --- CIII] Rest equivalent width of the emission lines of CIII] --- MgII Rest equivalent width of the emission lines of Mg II --- James Marcout, Patricia Bauer CDS 1994 Jun 30 Brian Boyle <BJB@ast-star.cam.ac.uk> UNKNOWN UNKNOWN Added table7 and table8 on 20 March 1997. These tables where prepared via OCR at CDS J_MNRAS_243_1.xml Galaxy redshift survey in a narrow strip crossing the Coma cluster J/MNRAS/243/390 J/MNRAS/243/390 Galaxy redshift survey in a Coma strip Galaxy redshift survey in a narrow strip crossing the Coma cluster I D Karachentsev A I Kopylov Mon. Not. R. Astron. Soc. 243 390 1990 1990MNRAS.243..390K Galaxies, optical Magnitudes, photographic Redshifts Regional catalog Surveys A list of galaxies brighter than 18m with the coordinates in the range RA=[10h42m,15h28m], Dec=[+28deg10min,+28deg10min] is presented. The list contains data on apparent photographic magnitude, angular, axial ratio and radial velocity for more than 300 objects. Emission and absorption line galaxies found show an essentially different character in their spatial distribution.
Redshift survey observations SeqNum Sequentiel Number --- RAh right ascension (hours) [1950] h RAm right ascension (minutes) min RAs right ascension (seconds) s DEd declination (degrees) [B1950] deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec mag Apparent magnitude mag AngDiam Angilar diameter in minutes of arc, measured on the blue POSS print along the major axis. arcmin Axratio Axial ratio for the galaxy image on the POSS blue print. --- Colour Indicator of colour of the object: + for red galaxies - for blue galaxies #0 for neutral colour --- Structure Object image structure flag: c = compact d = diffuse i = irregular. --- RV Radial velocity corrected for the solar motion with respect to the velocity centroid of the Local Group using the standard formula Vo = Vh + 300.sinl.cosb km/s u_RV Radial velocity quality flag : for unreliable velocity values * marks those radial velocities taken from elsewhere. --- e_RV Internal error of radial velocity measurement km/s Emission Emission line flag e = presence of emission lines a = absence of emission lines --- Notes NGC or IC catalogue number of galaxy. The objects marked with an asterisk are commented below number=1 Individual remarks: # 23. Probably belongs to Seyfert-1 type. # 37. Inner motion amplitude equals 192km/s # 41. Spectral signs of Seyfert-2. # 95. Declination is somewhat higher than the survey upper border. # 110. Haro 31. The value Vo=7883+/-86 (DuPuy 1970) is not confirmed by the Arecibo observations. # 229. The radial velocity is measured at 21 cm in Arecibo. According to Gregory (1975), Vo=+6654. # 253. Vo=+10867 (Moody & Kirshner 1988). # 256. Inner motion amplitude 210 km/s. # 257. Inner motion amplitude 400 km/s. # 321. Inner motion amplitude 133 km/s. # 358. According to Strauss & Huchra (1988), Vo=+17342+/-56. # 375. Instead of unreliable optical estimation Vo=+9300:+/-150 we give the velocity +9604+/-8km/s, measured at Arecibo. --- Joseph Florsch CDS 1994 Feb 10 UNKNOWN UNKNOWN Received from Pascal Fouque (1991) Reformatted and added Notes at CDS UNKNOWN UNKNOWN Notes: The following columns are not in the electronic version of table1: - Linear diameter of the galaxy A=a*Vo/H, expressed in kpc, the Hubble constant H being equal to 75 km/s/Mpc - Absolute magnitude M=m-5log(Vo/H)-25-{DELTA}m, where {DELTA}m=0.25+1.e-5*Vo accounts for average absorption value at high galactic latitudes and the K-correction for a galaxy of intermediate type. J_MNRAS_243_390.xml The APM galaxy survey. II. Photometric corrections. J/MNRAS/246/433 J/MNRAS/246/433 CCD photometry & APM parameters for galaxies The APM galaxy survey. II. Photometric corrections. S J Maddox G Efstathiou W J Sutherland Mon. Not. R. Astron. Soc. 246 433 1990 1990MNRAS.246..433M Galaxies, photometry The sequences for UKS fields 152 246 and 249 appear to be discrepant with the plate matching in the APM survey, and so may not be completely reliable.
CCD photometry and APM parameters for galaxies in the calibration sequences Name Galaxy name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec Bmag B magnitude mag Vmag V magnitude mag bJ bJ magnitude mag m APM magnitude mag Class Class, phi, as defined in Maddox et al. (1990) (Paper I) (-5000 flags merged images) number=1 A simple way of using all the APM parameters is to treat each of the levels, A_i_, and the peak density, P, as different measurements of the surface brightness profile, and use nine separate pairwise plots against magnitude. The radius of gyration is included as a tenth plot against magnitude. For each parameter p_i_ (where p_i_=A_i_, 1<=i<=8, p_9_=P, p_10_=K), a scatter plot of p_i_ against m is produced, the stellar locus is located as a function of magnitude, giving p_i_*(m). The final profile residual, phi, which is equivalent to the integrated difference between the particular image profile and the stellar profile at the same magnitude, is given by: phi = 1000log(sum(1to10){w_i_(m)[p_i_(m)-p_i_*(m)]^2^}), where w_i_ are the weighting factors, defined as w_i_=1/{delta}_i_^2^, with {delta}_i_ the estimated error in p_i_. --- Xpos X coordinate number=2 Position measured in 8 micron units from the centre of each plate 8um Ypos Y coordinate number=2 Position measured in 8 micron units from the centre of each plate 8um table3.tex TeX version of table3 Patricia Bauer CDS 1996 Sep 06 Steve Maddox <sjm@ast.cam.ac.uk> J_MNRAS_246_433.xml A homogeneous catalogue of quasar candidates found with slitless spectroscopy J/MNRAS/247/182 J/MNRAS/247/182 Catalogue of quasar candidates A homogeneous catalogue of quasar candidates found with slitless spectroscopy M Beauchemin E F Borra G Edwards Mon. Not. R. Astron. Soc. 247 182 1990 1990MNRAS.247..182B QSOs Spectroscopy This paper gives a list of all quasar candidates obtained from an automated computer search performed on 11 grens plates. The description of the main characteristics of the survey is given along with the latest improvements in the selection techniques. Particular attention has been paid to understanding and quantifying selection effects. This allows the construction of homogeneous samples having well-understood characteristics. The noteworthy aspect of our homogenization process is the correction that we apply to our probability classes in order to take into account the signal-to-noise differences; at a given magnitude, among plates of different limiting magnitudes. Since such homogeneous material is rare, this catalogue is of general interest. Each grens plate covers about 1 square degree with typical limiting magnitude of B~21. Data are given with all relevant quantities needed to understand the characteristics of the survey. We expect that over 100 of the 125 higher probability class candidates are quasars. A third of the ~400 lower probability objects should also be quasars. This material is well-suited to follow-up spectroscopy with fibre spectrographs.
Catalogue of quasar candidates Field Field name --- Id Grens reference number inside the field --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec u_DEs Uncertainty flag on DE number=1 *: Astrometry accurate to 0.6 arcsec **: Astrometry accurate to about 3 arcsec (evaluated on grens plates) --- Jmag J magnitude mag PrClass Probability class number=2 1: line s/n > 8 or 2 lines with s/n > 5 separated by at least 600 A 2: 6 < line s/n < 8 3: 5 < line s/n < 6 and colours more than 1 sigma away from the stellar main-sequence 4: no line and unusual colours (colour indices more than 2 standard deviations away from the stellas main-sequence locus) --- gb-gv gb-gv grens colour index mag gu-gb gu-gb grens colour index mag Dms Distance of the candidate from the nominal locus of the main sequence of stars number=3 0: the distance is between 0 and 1 standard deviation 1: the distance is between 1 and 2 standard deviations 2: the distance is between 2 and 3 standard deviations 3: the distance is greater than 3 standard deviations --- Sample Sample membership of the candidate --- EmLine Wavelength of the emission lines detected on grens plates for the highest probability classes candidates PC1 0.1nm Type Object type of some candidates number=4 Q = quasar, S = star --- z Emmision line redshift confirmed by slit spectroscopy --- Marie-Jose Wagner, Patricia Bauer CDS 1995 Jan 20 J_MNRAS_247_182.xml A 100-200 Mpc group of quasars J/MNRAS/249/218 J/MNRAS/249/218 Group of quasars A 100-200 Mpc group of quasars R G Clowes L E Campusano Mon. Not. R. Astron. Soc. 249 218 1991 1991MNRAS.249..218C QSOs Redshifts We have found evidence for a large, elongated group of at least ten quasars with largest dimension ~100-200h-1Mpc at z~1.3, in the direction of ESO/SERC field 927, which has the field centre (1950) 10h40m00s, 05deg00'00". There are probably further members that have not yet been observed. The morphology of the group seems to be like a clump, but there might be some sub-grouping on scales ~20h-1Mpc. The group is similar in size and number of quasars to that found by Crampton, Cowley & Hartwick (1989). The fact that two such groups are now known is evidence that the distribution of quasars is not so simple as was previously thought: at large scales (>10h-1Mpc) the majority of quasars may be distributed uniformly and at random, but rare, large groups also occur. The groups may be large physical structures, but a strong association with the large structures of galaxies seems doubtful.
S and W bands of quasars Band Band designation S= strong-lined, W=weak-lined --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec LSP Automated Quasar Detection (AQD) line-strength parameter --- z Redshift --- n_z Note on redshift number=1 Redshifts from Keable (1987) are identified by k --- Line Line --- EW Equivalent width 0.1nm Bj Bj magnitude mag Collation of redshifts data RAh Right Ascension (1950) h RAm Right Ascension (1950) min RAs Right Ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec z Redshift --- Bj Bj magnitude mag James Marcout, Simona Mei CDS 1995 Feb 28 UNKNOWN UNKNOWN Keypunched at CDS J_MNRAS_249_218.xml Main-sequence CCD photometry of the globular cluster omega Cen J/MNRAS/250/314 J/MNRAS/250/314 CCD photometry of omega Cen Main-sequence CCD photometry of the globular cluster omega Cen R G Noble R J Dickens J Buttress W K Griffiths A J Penny Mon. Not. R. Astron. Soc. 250 314 1991 1991MNRAS.250..314N Clusters, globular Photometry, CCD Positional data *** No Description Available ***
The SAAO color-magnitude data SAAO Number in SAAO observation (corresponds to Fig.2) --- V magnitude mag B-V color index mag The AAT color-magnitude data N Name --- x2 Position in AAT field O2 (Fig.6) pix y2 Position in AAT field O2 (Fig.6) pix x3 Position in AAT field O3 (Fig.6) pix y3 Position in AAT field O3 (Fig.6) pix x4 Position in AAT field O4 (Fig.6) pix y4 Position in AAT field O4 (Fig.6) pix V magnitude mag B-V color index mag Name SAAO name --- The faint colour-magnitude data from the WB, WR observations; x- and y-coordinates in field O1 N1 Number in AAT field O1 --- x1 Position in AAT field O1 pix y1 Position in AAT field O1 pix V magnitude mag B-V color index mag James Marcout, Francois Ochsenbein CDS 1994 Apr 15 UNKNOWN UNKNOWN Keypunched at CDS J_MNRAS_250_314.xml Flux densities at 8400MHz for a large sample of radio sources J/MNRAS/251/330 J/MNRAS/251/330 8400MHz flux densities for Southern sources Flux densities at 8400MHz for a large sample of radio sources A E Wright R M Wark E Troup R Otrupcek D Jennings A Hunt D J Cooke Mon. Not. R. Astron. Soc. 251 330 1991 1991MNRAS.251..330W Radio sources We present 8400-MHz flux densities for 1194 southern radio sources. The sources were selected from the Parkes 2700-MHz Survey to include all those stronger than 0.5 Jy at that survey's finding frequency of 2700 MHz. The new fluxes have an accuracy of about 8 per cent. corresponding to 0.05 Jy for a typical source. It is anticipated that the data will be useful in defining the high-frequency radio spectra of many sources as well as in pinpointing objects with which to improve the southern, astrometric absolute reference frame.
F(8400MHz) of Southern sources NAMEJ Source name derived from J2000 coordinates . Corr '*' for the 3 objets which have been corrected (see Note) . RAJh Right ascension, J2000 h RAJm Right ascension, J2000 min RAJs Right ascension, J2000 s DEJ- Declination J2000 (sign) . DEJd Declination J2000 deg DEJm Declination J2000 arcmin DEJs Declination J2000 arcsec OptId Optical identification of the source: Q = Quasar Q? = probable quasar QC = Quasar with continuous optical spectrum BLC= BL Lac object * = stellar object of neutral colour E,S,SC,N,D,DB,S0,SB = galaxy type G = galaxy of unspecified type HII= HII region SNR= Supernova Remnant X,Xs,etc = Blank fields(see PKScat90 database) . S8400 Newly measured 8400 MHz flux density Jy NAMEB Source name derived from B1950 coordinates . Francois Ochsenbein CDS 1993 Jan 05 J_MNRAS_251_330.xml CCD-photometry of galactic globular clusters - III. NGC 6171. J/MNRAS/252/357 J/MNRAS/252/357 Photometry of NGC 6171 CCD-photometry of galactic globular clusters - III. NGC 6171. F R Ferraro G Clementini F Fusi Pecci R Buonanno Mon. Not. R. Astron. Soc. 252 357 1991 1991MNRAS.252..357F Clusters, globular Photometry, CCD B and V CCD photometry is presented for 1565 stars in the low-concentration globular cluster NGC6171=M107
Non-variable stars in the bright sample (V=<18) Non-variable stars in the faint ample (V>18) N Identification number --- Vmag V magnitude mag B-V B-V colour mag X X position (1 pixel = 0.35 arcsec) pix Y Y position (1 pixel = 0.35 arcsec) pix Patricia Bauer CDS 1994 Sep 21 Francesco Ferraro <astbo3::ferraro> J_MNRAS_252_357.xml Interferometer phase calibration sources. I. The region 35{deg}<={delta}<=75{deg}. J/MNRAS/254/655 J/MNRAS/254/655 Interferometer phase calibration sources. I Interferometer phase calibration sources. I. The region 35{deg}<={delta}<=75{deg}. A R Patnaik I W A Browne P N Wilkinson J M Wrobel Mon. Not. R. Astron. Soc. 254 655 1992 1992MNRAS.254..655P Radio sources We present a catalogue of 800 compact radio sources in the declination range 35deg<{delta}<75deg whose positions have been measured to an rms accuracy of ~12milliarcsec with the VLA. They are primarily intended for use as phase reference sources for the Jodrell Bank MERLIN but they will also be suitable phase calibrators for the VLA and the VLBI networks.
List of phase calibrators. List of sources found in the survey which are not suitable as calibrators. Bname Source name derived from B1950 coordinates --- Jname Source name derived from J2000 coordinates --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec S8.4GHz Total flux density at 8.4GHz mJy Code Code number=1 P: primary calibrator with >95% of their flux density contained in an unresolved component S: secondary calibrators up to 20% resolved on the longest baselines but with point-dominated structure D: double source --- Com Comments on structure --- James Marcout, Patricia Bauer CDS 1997 May 22 UNKNOWN UNKNOWN Prepared via OCR at CDS. * 15-Jul-1997: Thanks are due to H. Andernach for communicating the errors he detected, and a corrected position (derived from Taylor et al's 1996ApJS..107...37T VLA observations) for the source B0256+424 * 11-Nov-1997: further errors reported by Browne et al. to H. Andernach to be published in "Interferometer phase calibration sources II" for B1705+456 and B1817+502 J_MNRAS_254_655.xml Proper motions from Schmidt plates. II. The Hyades. J/MNRAS/257/257 J/MNRAS/257/257 Proper motions from Schmidt plates. II. The Hyades. Proper motions from Schmidt plates. II. The Hyades. N Reid Mon. Not. R. Astron. Soc. 257 257 1992 1992MNRAS.257..257R astrometry open clusters and associations: individual (Hyades) stars: luminosity function, mass function surveys techniques: photometric We have used COSMOS scans of photographic plates taken by the Palomar Oschin Schmidt telescope (as part of the original Palomar Sky Survey) and by the UK Schmidt telescope to obtain proper motions for ~ 450 000 stars within a 112-degree region covering part of the Hyades cluster. With epoch differences of 33 to 37 yr, we have obtained proper motions accurate to 6-12 mas/yr and have identified 393 candidate Hyads to a limiting magnitude of Mv ~ +15.5, including at least two new white dwarf candidates. The main-sequence luminosity function determined from our sample is similar to that defined by local field stars, with a broad maximum at Mv ~ +12. Deriving distances from mu u, the proper motion towards the convergent point, and the space velocity determined by Gunn et al., we find stars with motions consistent with membership at distances of more than 15pc from the cluster centre. Moreover, both the line-of-sight and surface density distributions show evidence for significant mass segregation - indeed, the overall proper motion distribution suggests a tight core centred within a much broader distribution. We derive a total mass of 410-480Sun and a gravitational binding radius of ~ 10.5pc.
Candidate Hyads Seq Running number --- Note Indicator: G = Galaxy, * = near bright stars. When this column is not blank, positions and colors are not listed. --- Pr Membership indicator: 1 = probable member based on (Mv,(V-I)K) relation 2 = probable non-member based on (Mv,(V-I)K) relation 3 = probable non-member based on preliminary reduction of CCD data --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec pmRA Proper motion in right ascension (* cos(DE)) arcsec/yr pmDE Proper motion in declination arcsec/yr pmU Proper motion directed towards the Hyades convergent point (around RA=98deg,DE=+6deg) arcsec/yr pmT Proper motion transverse to convergent point arcsec/yr V apparent magnitude mag B-V color index mag Mv Absolute magnitude mag WD White Dwarf indication --- Cross-references Seq Running number as in table8 --- vB van Bueren number (see Acronyms) Inst. Netherlands 11, 385, 1952) --- vA van Altena number (see Acronyms) --- HA Hanson number (see Acronyms) --- LP Luyten name (see Acronyms) 48"-Schmidt Telescope, LIX, Minesota Univ., 1981) --- LH Leggett & Hawkins (see Acronyms) --- HG Giclas designation (see Acronyms) --- Leiden Leiden number from Pels et al. (see Acronyms) --- Ha indicates whether the star is included in Stauffer et al. (ApJ 374, 142, 1991) --- GGZG indicated whether the star is included in Griffin et al. (AJ 96, 172, 1988) --- CCD Photometric sequences Id1 First designation (see Acronyms) --- Id2 Second designation (see Acronyms) This field is non-blank in app-c only --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec V Magnitude mag B-V color index mag V-R color index mag V-I color index mag Appendix B: Giclas stars Appendix C: Hanson stars Appendix D: Leiden (Pels et al.) stars Appendix E: Luyten stars Appendix F: Leggett & Hawkins stars Id1 First designation number=1 Acronyms: The acronyms are: HG = Giclas (Lowell Obs. Bull. 5, 257, 1962) vB = van Bueren (Bull. Astr. Inst. Netherlands 11, 385, 1952) vA = van Altena number (AJ 74, 2, 1969) HA = Hanson number (AJ 80, 379, 1975) LP = Luyten (Proper Motion Survey with 48"-Schmidt Telescope, LIX, Minesota Univ., 1981) LH = Leggett & Hawkins number (MNRAS 238, 145, 1989) Leiden = Pels et al. (A&A 43, 423, 1975) --- Id2 Second designation (1) This field is non-blank in app-c only --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) - DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec V Magnitude mag B-V color index mag pmRA Proper motion (*cos(DE)) arcsec/yr pmDE Proper motion in DE arcsec/yr M.J. Wagner, Francois Ochsenbein CDS 1994 Mar 21 UNKNOWN UNKNOWN Keypunched at CDS J_MNRAS_257_257.xml The cluster of galaxies SC2008-57(A3667) J/MNRAS/259/233 J/MNRAS/259/233 The cluster of galaxies SC2008-57 The cluster of galaxies SC2008-57(A3667) L Sodre H V Capelato J E Steiner D Proust A Mazure Mon. Not. R. Astron. Soc. 259 233 1992 1992MNRAS.259..233S catalogs galaxies: clusters: general galaxies: distances and redshifts galaxies: luminosity function, mass function galaxies: photometry (Abstract of the paper) We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.
Galaxy catalogue of the cluster of galaxies SC2008-57 (A3667) N galaxy number --- RAh right ascension (hours) (B1950) h RAm right ascension (minutes) min RAs right ascension (seconds) s DE- declination sign . DEd declination (degrees) (B1950) deg DEm declination (minutes) arcmin DEs declination (seconds) arcsec X Cartesian coordinate X measured over the plate arcsec Y Cartesian coordinate Y measured over the plate arcsec b25 isophotal bj magnitude given by pixels brighter than 25 mag/arcsec^2 mag u_b25 uncertainty flag of b25 magnitude due to overlapping --- Vhelio heliocentric radial velocity km/s u_Vhelio uncertainty flag of Vhelio --- e_Vhelio error of Vhelio km/s r_Vhelio code for the reference of Vhelio See the caption of Table 3 of the paper. --- NOTES notes on the velocity determination or on the galaxy identification See the caption of Table 3 of the paper. --- t3.tex LaTeX Table 3 Koichi Nakajima CDS 1993 Nov 04 UNKNOWN UNKNOWN The catalogue was provided by courtesy of L. Sodre to H. Andernach; it was numbered A108 in H. Andernach's "List of Astronomical Catalogues and Documents kindly provided on request by various authors" 08-Nov-1993: First archived in J/MNRAS/259/233. __-Jan-1994: Amended, removing a supplementary file following the author's comment. (The date of the latest archive, see the date of each file.) UNKNOWN UNKNOWN Notes: * In order to execute LaTeX of "t3.tex", a definition file "macros.tex" is needed in which at least definitions of \kmsec, \double, \etal are included. Comment from the author (Sodre L.): The galaxy numbers in the Table 2 of the paper were not those from the Table 3. The correct numbers are 065, 086, 087, 097, 100, 120, respectively. J_MNRAS_259_233.xml Double star CCD astrometry and photometry J/MNRAS/259/563 J/MNRAS/259/563 Double star CCD astrometry and photometry Double star CCD astrometry and photometry A N Argue P S Bunclark M J Irwin P Lampens D Sinachopoulos P A Wayman Mon. Not. R. Astron. Soc. 259 563 1992 1992MNRAS.259..563A astrometry binaries: close binaries: visual techniques: image processing *** No Description Available ***
v >= 9 mag. and rho < 5" v >= 9 mag. and rho >= 5 " 8 <= v < 9 mag. and rho < 5 " Nr an internal number --- IDS Identification in the "Catalogue of the Components of Double and Multiple stars" (CCDM, Dommanget 1985; equinox 1900) --- Name Double star designation --- t Epoch of observation; yr theta Position angle of component B relative to A (N through E); deg rho Angular separation rho of A,B arcsec d Distance between the two positions derived for B relative to A, giving an estimate of the precision arcsec mvA Apparent V magnitude of the A component mag mvB Apparent v magnitude of the B component mag sv FWHM of the derived PSF for the v images (see 3; unit 0.1 arcsec); 0.1arcsec mrA Apparent R magnitude of the A component; mag mrB apparent R magnitude of the B component mag sR FWHM of the derived PSF for the R magnitude 0.1arcsec SD_V Standard deviation of a V magnitude as determined by the Carlsberg Automatic Meridian Circle on the mountain. No data are available for Star No. 4451. mag Francois Ochsenbein CDS 1994 Jan 31 UNKNOWN UNKNOWN 19-Feb-1993 Version 31-Jan-1994: removed the LaTeX files from "File Summary", and modified the Byte-by-byte Description for NULL values J_MNRAS_259_563.xml The quasar luminosity function from a variability-selected sample J/MNRAS/260/202 J/MNRAS/260/202 Quasar luminosity function The quasar luminosity function from a variability-selected sample M R S Hawkins P Veron Mon. Not. R. Astron. Soc. 260 202 1993 1993MNRAS.260..202H cosmology: observations quasars: general A sample of quasars is selected from a 10-yr sequence of 30 UK Schmidt plates. Luminosity functions are derived in several redshift intervals, which in each case show a featureless power-law rise towards low luminosities. There is no sigh of the 'break' found in the recent UVX sample of Boyle, Shanks & Peterson. It is suggested that reasons for the disagreement are connected with biases in the selection of the UVX sample. The question of the nature of quasar evolution appears to be still unresolved.
List of quasars Name Quasar name number=1 a: FOCAP sample, b: bright sample --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec Bmag B magnitude at minimum mag U-B U-B colour mag Signi Significance parameter number=2 s is the measure of the significance of the difference between the maximum and minimum magnitudes --- z Redshift --- MB Absolute B magnitude at minimum mag Marie-Jose Wagner, Patricia Bauer CDS 1994 Dec 05 UNKNOWN UNKNOWN Keypunched at CDS J_MNRAS_260_202.xml The ROSAT Wide Field Camera all-sky survey of extreme-ultraviolet sources - I. The Bright Source Catalogue J/MNRAS/260/77 J/MNRAS/260/77 The ROSAT Wide Field Camera all-sky survey of The ROSAT Wide Field Camera all-sky survey of extreme-ultraviolet sources - I. The Bright Source Catalogue K A Pounds D J Allan C Barber M A Barstow D Bertram G Branduardi-Raymont G E C Brebner D Buckley G E Bromage R E Cole M Courtier A M Cruise J L Culhane M Denby D O Donoghue E Dunford I Georgantopoulos C V Goodall P M Gondhalekar J A Gourlay A W Harris B J M Hassall C Hellier S Hodgkin R D Jeffries B J Kellett B J Kent R Lieu C Lloyd P A Mcgale K O Mason L Matthews J P D Mittaz C G Page G S Pankiewicz C D Pike T J Ponman E M Puchnarewicz J P Pye J J Quenby M J Ricketts S R Rosen A E Sansom S Sembay S Sidher M R Sims B C Stewart T J Sumner R J Vallance M G Watson R S Warwick A A Wells R Willingale A P Willmore G A Willoughby D Wonnacott Mon. Not. R. Astron. Soc. 260 77 1993 1993MNRAS.260...77P X-ray sources Table 1 gives the coordinates (equinox J2000.0) of 384 bright EUV sources detected in the WFC survey. These should be referred to, according to the IAU convention, by the suitably truncated RA and Dec. Thus, the first source in the Table is RE J0003+433, a ROSAT EUV source at 00h 03m and +43deg 35'. Count rates and 1sigma errors are given for each of the survey filters, in counts per kilosecond. Upper limits are indicated by "-" in the error column and are 3sigma above the local background.
The Bright Source Catalogue RAh Right Ascension J2000 (hours) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). h RAm Right Ascension J2000 (minutes) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). min RAs Right Ascension J2000 (seconds) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). s DE- Declination J2000 (sign) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). --- DEd Declination J2000 (degrees) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). deg DEm Declination J2000 (minutes) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). arcmin DEs Declination J2000 (seconds) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). arcsec S1a Count rates in filter S1 (90-206eV) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). ct/ks e_S1a mean error on S1a number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). ct/ks S2a Count rates in filter S2 (62-110eV) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). ct/ks e_S2a mean error on S2a number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). ct/ks Name1 Possible counterpart number=1 Information on possible counterparts within the 99.9% WFC position error circle is given. The first counterpart listed is thought to be the most likely identification from the information available in existing catalogues and optical follow up work on some sources (Mason et al., 1992). Extensive use was made of the CDS SIMBAD database, particularly for obtaining information on multiple names for objects. Two names are usually given for the first counterpart; normally a common or variable star name, followed by an HD or WD (McCook and Sion, 1987) number, where available. One name is generally given for other objects within the 99.9% error circle. Information on many of the object names used here can be found in Fernandez et al. (1983). Object types for the counterparts are given; spectral type classifications for the same object, but from different catalogues, are all listed, separated by slashes. For more detailed and accurate spectral type classifications for active binaries, see Strassmeier et al. (1988). The magnitudes of the counterparts are given (usually in the V-band unless B magnitudes are indicated by a "B"). They are meant only as a rough guide, since they are drawn from a variety of catalogues, and many of these objects are optically variable. It is important to note that visual or spectroscopic binary companions can rarely be ruled out as the source of EUV emission. --- Name2 Possible counterpart number=1 Information on possible counterparts within the 99.9% WFC position error circle is given. The first counterpart listed is thought to be the most likely identification from the information available in existing catalogues and optical follow up work on some sources (Mason et al., 1992). Extensive use was made of the CDS SIMBAD database, particularly for obtaining information on multiple names for objects. Two names are usually given for the first counterpart; normally a common or variable star name, followed by an HD or WD (McCook and Sion, 1987) number, where available. One name is generally given for other objects within the 99.9% error circle. Information on many of the object names used here can be found in Fernandez et al. (1983). Object types for the counterparts are given; spectral type classifications for the same object, but from different catalogues, are all listed, separated by slashes. For more detailed and accurate spectral type classifications for active binaries, see Strassmeier et al. (1988). The magnitudes of the counterparts are given (usually in the V-band unless B magnitudes are indicated by a "B"). They are meant only as a rough guide, since they are drawn from a variety of catalogues, and many of these objects are optically variable. It is important to note that visual or spectroscopic binary companions can rarely be ruled out as the source of EUV emission. --- Type Counterpart type number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). --- Mag Counterpart magnitude number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). mag n_Mag Note on the Counterpart magnitude number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). --- Comments See Note number=2 The column headed "comments" contains information regarding the counterparts as detailed below: E: Exosat detection within WFC error circle. I: IUE target within WFC error circle (not necessarily a detection). pm: High proper motion star, from the Luyten catalogue of stars with proper motions >0.5 arcseconds per year (Luyten, 1976). N: Nearby stars, from the Gliese and Jahreiss (1969,1979,1991) catalogues. A: Active star or star system (mostly from the Strassmeier et al. catalogue of chromospherically active binary stars). The "A" flag is not given for RS CVn and BY Dra systems, or where the spectral type indicates emission (e.g. dMe). (B): The most probable counterpart is a known binary, or has one or more sources nearby, within the error circle, with the same name, but a different qualifying letter at the end, usually implying a visual binary or multiple star system. The source(s) of EUV emission are not always clear in these cases. V*: Variable star, from the general catalogue of variable stars (GCVS), either directly or via the SIMBAD database. EI: Einstein IPC detection within WFC error circle. H: Einstein HRI detection within WFC error circle. N(H)= Interstellar hydrogen absorption column, in units of 10^20 cm-2, estimated from the maps of Stark et al. (1992; available for _delta_> -40deg) for extragalactic counterparts within the error circles. Generally we do not expect to detect extragalactic sources through a column greater than N(H)~2. (C): Designates another counterpart in the error circle, which has the same name, but different extension letter to the first counterpart. b: Blue star, generally from the master list of non-stellar sources (Dixon, 1970), or from references given in the SIMBAD database. HEAO: HEAO-A1 detection (Wood et al., 1984). IDP: ROSAT WFC optical identification programme (Mason et al., 1992) with activity/non-activity represented by "A" and "nonA" respectively. "IDPn" indicates no identification yet found from spectroscopic search of EUV error circle. The final three columns in Table 1 give the WFC 90% confidence position error circle radius (arcsecs); the counterpart offset from the EUV source position (arcsecs), and the catalogue from which the counterpart position was taken. Sources for which there is note below are marked with a "R" symbol at the end of the entry. The catalogue names are abbreviated as listed below (following notes on individual sources). --- R90 90%-confidence position error circle radius number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). arcsec DR Counterpart offset from EUV source position number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). arcsec Cat Catalogue from which the counterpart position was taken number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). --- Rem 'R' for Notes (see below) number= individual sources ('R' in column 129): RE 0044+093: New fast rotating single star radio source (Bromage et al., in preparation). RE 0116-022: AY Cet is an active close binary with a WD companion (Strassmeier et al., 1988) and a 57 day orbit. The WD is not expected to contribute to the EUV flux. RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission coming from 40 Eri C, the dMe flare star (Cash et al., 1980). All three components could be contributing to the EUV flux. RE 0447-275: Identification is with a newly discovered dMe star, the fainter companion of a close visual pair; this has subsequently been discovered to be a flare star (Bromage, 1992). RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude, A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows a rise towards short wavelengths, indicative of a hot white dwarf companion (Hodgkin et al., 1992). Other catalogued stars in the WFC error circle include the 5th magnitude A9IV star KW Aur, and the 11th magnitude star BD+32 922B, which are both unlikely to contribute to the detected EUV flux. RE 0532-030: Star identified may be HBC97 (dKe) but this association is uncertain because of position discrepancies. RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new dMe flare star. See Bromage (1992). RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no reported variations in radial velocity or photometry whereas star B (G6V) has variable RV and photometric variability. Following the IDP discovery of chromospheric activity (Mason et al., 1992) it seems very likely that star B is the EUV emitter and is probably an SB1 RSCVn binary. RE 0631+500: The dMe star discovered in the optical identification programme now appears (but not named) in the latest version of the Gliese catalogue (1991) as an M0 star with V=11.09 mag. RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter count rate was enhanced by a flare event on 1990 Oct 03 (Bromage, 1992). RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b). RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a subdwarf in the Palomar Green survey (Green et al., 1986 - hereafter PG), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th magnitude K giant in the WFC error circle, which is likely to be a chance coincidence. RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary (Jomaron et al., 1992). RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a hot subdwarf (sdB) in the PG survey and more recently shown to be a possible hot DA white dwarf (Sansom et al., 1992). Because of the low signal-to-noise data the optical classification of this star is still uncertain, as indicated by the colon after the spectral type in table 1. RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf Also in the EUV source error circle is probably too cool to be detected. RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star _beta_ Crt, the likely source of EUV emission has been shown to be a DA white dwarf companion _beta_ Crt B (Fleming et al., 1991), which is a spectroscopic binary companion to _beta_ Crt. RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992). RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a hot subdwarf (sdOB) in the PG survey, and more recently shown to be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992). RE 1255+255: The variable star IN Com, within the WFC error circle, is very close to the centre of the planetary nebula LT5. IN Com is a triple system consisting of an 8.7th magnitude, G5 III star with active chromosphere and a low mass, binary companion, plus an outer, hot subdwarf (Malasan et al., 1991). The G star is the most likely source of EUV emission, but emission from the other components cannot be ruled out. RE 1307+535: Identified as probable new AM Her system, with the shortest known period in the class (Osborne et al., 1992). RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later Optically identified by Remillard et al. (1989). RE 1603-574: _iota_ Nor consists of a group of several 5th magnitude mid-A stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has now been shown to be a 6-day period double-lined spectroscopic binary active G star and candidate RSCVn binary (Bromage, 1992). RE 1625-490: The optical identification has been made independently by Cutispoto et al. (1992) from an optical follow up programme of serendipitous EXOSAT sources; the object does not show any evidence of binarity. RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et al., 1992). RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently shown to be a hot DA white dwarf (Sansom et al., 1992). RE 1833+514: The famous prototype of the BY Dra class of spotty active stars; the S2 flux was enhanced by a flare (Barstow et al., 1991). RE 1938-461: Identified as new AM Her system (Buckley et al., 1992). RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a flare (Bromage, 1992). RE 2047-363: A newly discovered very fast rotating single dwarf star, Nicknamed "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by a long-lived flare, and variability of activity occurred in both filters. RE 2147-160:_delta_ Cap: the visual companions of this 3rd magnitude peculiar A star binary have been ruled out as possible EUV counterparts by CCD photometry and high-resolution spectroscopy, leaving the likely counterpart as the hidden binary companion of _delta_ Cap itself (probably a mildly active late type star). (Wonnacott et al., 1992). RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the common proper-motion WD companion is too cool to contribute to the EUV flux, but the derived age of the system makes G1841A one of the oldest known active star systems (Jeffries and Bromage, 1992). RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes were enhanced by flares during the survey coverage (Bromage, 1992). --- Francois Ochsenbein CDS 1993 May 29 Thanks are due to Dr Mike Watson for e-mailing the LaTeX files. "DeTeX" was performed at CDS, and the insertion of the 'J' for truncated IAU-style designation was added in the text. J_MNRAS_260_77.xml CCD photometry of two young Large Magellanic Cloud clusters: NGC 2004 and 2100 J/MNRAS/260/782 J/MNRAS/260/782 CCD photometry of two young Large Magellanic CCD photometry of two young Large Magellanic Cloud clusters: NGC 2004 and 2100 L A Balona M Jerzykiewicz Mon. Not. R. Astron. Soc. 260 782 1993 1993MNRAS.260..782B Cepheids galaxies: star clusters Magellanic Clouds stars: early-type In this paper we present results of CCD UBV photometry of stars in two young LMC clusters: NGC 2004 and 2100. A comparison of recent CCD investigations of these clusters shows large zero-point discrepancies.
CCD magnitudes and colours of stars in the two clusters Cluster Cluster name --- N Sequence number (relative to cluster) --- X X position pix Y Y position pix V V magnitude mag B-V B-V colour mag U-B U-B colour mag M.J. Wagner, Francois Ochsenbein CDS 1994 Mar 22 UNKNOWN UNKNOWN Keypunched at CDS J_MNRAS_260_782.xml The radio and optical properties of the z<0.5 BQS quasars J/MNRAS/263/425 J/MNRAS/263/425 Low-z BQS Quasars The radio and optical properties of the z<0.5 BQS quasars P Miller S Rawlings R Saunders Mon. Not. R. Astron. Soc. 263 425 1993 1993MNRAS.263..425M galaxies: active quasars: general radio continuum: galaxies *** No Description Available ***
Optical positions Name Schmidt & Green catalogue identifier --- Opt Code representing source of new optical position number=1 Code for new optical position. no code means position is same as in Schmidt & Green (1983). A Argyle & Eldridge (1990) C Clements (1981) D Clements (1983a) E Clements (1983b) G This work: GASP measurement H Hewitt & Burbidge (1987) I This work: IoA Coradograph measurement S Green, Schmidt & Liebert (1986) --- RAh Right Ascension 1950.0 h RAm Right ascension 1950.0 min RAs Right ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec Radio data Name Schmidt & Green catalogue identifier. --- l_F4.86 Limit flag on total 4.86-GHz flux density --- F4.86 Total 4.86-GHz flux density, from Kellermann (1989) (D-array observations) except where indicated in the text. mJy RAh Right ascension 1950.0 of central component h RAm Right ascension 1950.0 of central component min RAs Right ascension 1950.0 of central component s DE- Declination sign --- DEd Declination 1950.0 of central component deg DEm Declination 1950.0 of central component arcmin DEs Declination 1950.0 of central component arcsec l_PB4.86 limit flag on 4.86-GHz peak brightness --- PB4.86 4.86-GHz peak brightness of the central component in from the high-resolution (VLA A-array) maps. mJy n_PB4.86 A * symbol denotes a brightness which has been derived from a brightness at 1.5GHz with {alpha}= 0.7 --- Class Radio-structure classification number=1 Radio-structure classification D denotes sources which are large radio sources, most of which are double-lobed and have terminal hotspots on one or both sides of the nucleus (the so-called "classical doubles" or "FR-IIs") but all of which are known from lower resolution maps to have linear sizes much larger than a typical galaxy size. P denotes sources, other than those of class 'D', which have R>0.7 E denotes sources, other than those of class 'D', which have R<0.7 Q denotes sources, other than those of class 'E', which were undetected in the D-array or the A-array observations, or which had very low fluxes in D-array. ? symbol marks a classification which is subject to some reasonable doubt --- theta Angular size arcsec Radio data from the literature Name Schmidt & Green catalogue identifier. --- F151 Flux density at 151MHz number=1 Fluxes from 4C references have been corrected as necessary for average resolution effects, converted to the Baars (1977) flux scale and, by use of a spectral index of 0.7, converted from 178MHz to 151MHz. Jy r_F151 References code (see table4c) --- l_F408 limit flag on flux density at 408MHz --- F408 Flux density at 408MHz Jy r_F408 References code (see table4c) --- l_F1490 limit flag on flux density at 1490MHz --- F1490 Flux densities at 1490 MHz (or 1415 MHz) mJy r_F1490 References code (see table4c) --- OF1490 Resolution of observations when several resolutions were used arcsec l_F4860 limit flag on flux density at 4860 MHz --- F4860 Flux density at 4860 MHz mJy r_F4860 References code (see table4c) --- OF4860 Resolution of observations when several resolutions were used arcsec F8400 flux density at 8400 MHz mJy r_F8400 References code (see table4c) --- l_F14900 limit flag on flux density at 14900 MHz --- F14900 Flux density at 14900 Mhz (or 14800 MHz) mJy r_F14900 References code (see table4c) --- OF14900 Resolution of observations when several resolutions were used arcsec ref References to lower-resolution maps. --- Spectral indices Class Radio-structure class. --- Name Schmidt & Green catalogue identifier. --- l_alpha limit flag on spectral index --- alpha Spectral Index between frequencies {nu}_1_ and {nu}_2_, for {nu}_1_ in the next column and {nu}_2_=4860MHz (except PG0838+770, for which {nu}_2_=14900MHz). --- Nu1 Lower frequency in MHz. MHz Ref References to flux densities, for determination of {alpha}, in format (S_{nu}_1_, S_{nu}_2_); and notes on this calculation. --- References for table4a and table4b Abbr Abbreviation --- Surey Survey title --- Ref Reference --- Obs Observation epoch(s) --- Resol Resolution(s) --- Patricia Bauer CDS 1994 Sep 22 J_MNRAS_263_425.xml On the giant, horizontal and asymptotic branches of galactic globular clusters - V. CCD photometry of NGC 1261. J/MNRAS/264/273 J/MNRAS/264/273 CCD photometry of NGC 1261 On the giant, horizontal and asymptotic branches of galactic globular clusters - V. CCD photometry of NGC 1261. F R Ferraro G Clementini F Fusi Pecci E Vitiello R Buonanno Mon. Not. R. Astron. Soc. 264 273 1993 1993MNRAS.264..273F Clusters, globular Photometry, CCD globular clusters: individual (NGC 1261) Hertzsprung-Russell (HR diagram) stars: abundances stars: evolution BV CCD photometry is presented for 3352 stars (18 variables) in the globular cluster NGC 1261.
NGC 1261 C 0310-554 03 11.7 -55 14
Final magnitudes, colours & positions for 3334 stars No Sequence number --- Vmag V magnitude mag B-V B-V color index mag Xpos X position number=1 The coordinates refer to the cluster center (1 pixel = 0.47 arcsec) pix Ypos Y position number=1 The coordinates refer to the cluster center (1 pixel = 0.47 arcsec) pix Patricia Bauer CDS 1996 Aug 23 F.R. Ferraro <FERRARO@astbo3.bo.astro.it> J_MNRAS_264_273.xml Observations of quasars in ESO/SERC field 927 J/MNRAS/266/317 J/MNRAS/266/317 Quasars in ESO/SERC field 927 Observations of quasars in ESO/SERC field 927 R G Clowes L E Campusano Mon. Not. R. Astron. Soc. 266 317 1994 1994MNRAS.266..317C galaxies: clusters: general large-scale structure of universe quasars: absorption lines quasars: emission lines quasars: general We present the spectroscopic observations of 56 quasars that were discovered by AQD (Automated Quasar Detection) in a field of ~25.3deg2, centred at (1950) RA l0h40m00s, Dec. 05deg00'00". These observations, with the CTIO 4-m telescope, led to the discovery by Clowes & Campusano of a large group of quasars with size ~100-200h^-1^Mpc at z~1.3. Quasars of particular interest are noted, including one that is a BAL quasar with z~1.78.
A summary of the observations of the 56 candidates that were confirmed as quasars. RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec RAh2000 Right ascension (2000) h RAm2000 Right ascension (2000) min RAs2000 Right ascension (2000) s DEd2000 Declination (2000) deg DEm2000 Declination (2000) arcmin DEs2000 Declination (2000) arcsec Date Date of observation --- Int Integration time s Band Band number=1 'S' for strong-lined, 'W' for weak-lined --- Bj Bj magnitude mag z redshift --- EW Equivalent width 0.1nm n_EW Note on equivalent width number=2 Identification of strongest emission lines: (1) Ly-alpha lambda 1216 +Nv lambda 1240; (2) C IV lambda 1549; (3) C III lambda 1909; (4) Mg II lambda 2798. --- Com Comments --- James Marcout, Patricia Bauer CDS 1995 Feb 14 UNKNOWN UNKNOWN Keypunched at CDS J_MNRAS_266_317.xml The variability of optically selected quasars J/MNRAS/268/305 J/MNRAS/268/305 Variability of optically selected quasars The variability of optically selected quasars I M Hook R G McMahon B J Boyle M J Irwin Mon. Not. R. Astron. Soc. 268 305 1994 1994MNRAS.268..305H Magnitudes QSOs Redshifts quasars: general The variability properties of a sample of ~300 optically selected quasars near the South Galactic Pole (SGP) have been studied over a baseline of 16 years using a series of twelve UK Schmidt Telescope B_J_ plates at seven epochs. In this sample there is a correlation between variability and both quasar luminosity and redshift, at greater than the 99 per cent significance level. Quasars of high luminosity show significantly less variability than those with low luminosity, the rms variation ranging from about 0.25mag at M_B_=-23 to 0.1mag at M_B_=-28. The observed trends can be explained by an intrinsic dependence of quasar variability on luminosity combined with the effects of time dilation, and have implications for quasar samples selected by variability or multicolour techniques. The change in the slope of the n(m) relation at the break can be less pronounced in variability-selected samples. Our results can be used to test models for the origin and reprocessing of the continuum emission in quasars.
Positions, redshifts, mean apparent Bj magnitudes and variability index for the SGP sample RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec z Redshift --- Bj Mean apparent B_J_ magnitude mag sigmaV Variability index sigma_V_ number=1 sigma_v_=1/(Ne-1)*[sum(i=1 to Ne)(|m_i_-<m>|)]*sqr(pi/2) where Ne is the number of epochs at which the quasar was visible on the plate and m_i_ the magnitude of the quasar at the epoch i --- Ref Reference number=2 References: 1: Boyle et al., 1985MNRAS.216..623B 2: Boyle et al., 1990, Cat. <J/MNRAS/243/1> 3: Burbidge et al., 1977ApJ...218....1B 4: Campusano, 1986IAUS..119...49C 5: Campusano, 1991AJ....102..502C 6: Hazard et al., 1986Natur.322...38H 7: Hazard et al., 1986MNRAS.223...87H 8: Hazard et al., 1987ApJ...323..263H 9: Hazard & McMahon, in prep. 10: Jauncey et al., 1984ApJ...286..498J 11: Morris et al., 1991AJ....102.1627M 12: Pocok et al., 1984MNRAS.210..373P 13: Savage et al., 1985MNRAS.213..485S 14: Smith et al., 1981MNRAS.195..437S 15: Trew et al., 1982MNRAS.200..785T 16: Wampler, 1985ApJ...296..416W 17: Warren et al., 1987Natur.330..453W 18: Warren et al., 1987Natur.325..131W 19: Warren et al., 1991, Cat. <J/ApJS/76/23> --- Note Notes number=3 a: z < 0.3 b: <m> > 21.0 c: <M_B_> > -23.0 d: classified as non-stellar by APM e: merged with another image on reference plate f: object appeared at fewer than 5 independent epochs g: photometry on plate J14545 affected by fireball --- James Marcout, Patricia Bauer CDS 1997 Mar 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. Corrections made on 21-Jul-1997: In line 297: "1 1 11.81" corrected in "1 1 01.81" In line 298: "1 1 14.08" corrected in "1 1 04.08" In line 299: "1 1 18.24" corrected in "1 1 08.24" In line 303: "1 1 20.67" corrected in "1 2 00.67" In line 304: "1 1 23.81" corrected in "1 2 03.81" J_MNRAS_268_305.xml Compact radio cores in radio galaxies. J/MNRAS/268/602 J/MNRAS/268/602 Compact radio cores in radio galaxies. Compact radio cores in radio galaxies. P A Jones W B McAdam J E Reynolds Mon. Not. R. Astron. Soc. 268 602 1994 1994MNRAS.268..602J Galaxies, radio Interferometry This catalog contains compact core fluxes for a list of 175 southern radio galaxies, measured with the Parkes-Tidbinbilla Interferometer (PTI, Norris et al. 1988ApJS...67...85N) on a single 275 km baseline at 2.3 GHz and 8.4 GHz. The sample consists of large angular size ( > 0.5 arcmin) steep spectrum sources from Jones & McAdam (1992ApJS...80..137J) observed to determine the fraction of flux contained in compact (VLBI-scale) cores. Of the 172 sources observed at 2.3 GHz (100 milliarcsec fringe spacing), 63 had cores detected and upper limits were determined for the remaining 109. Of the 88 sources observed at 8.4 GHz (30 milliarcsec fringe spacing), 38 had cores detected and 50 have upper limits. A comparison of the detections and upper limits at the two frequencies shows that the cores have flat or inverted spectra. The core fluxes quoted here may vary by around 20 % if there is structure on the scale of the fringe spacing and the cores are probably intrinsically variable.
Compact Radio Cores in Radio Galaxies (Dec < -30d) name Name of source, from B1950 position number=1 This column gives the name of the source, comprised of the hours and minutes of right ascension, the sign of the declination, the degrees truncated to the nearest tenth of a degree, and a capital letter (if the position code is ambiguous). The position used is the radio centroid in B1950 coordinates from the 843 MHz MOST data (Jones & McAdam 1992ApJS...80..137J) so the names may differ in some cases from the source names in the Molonglo Reference Catalogue (MRC, Large et al. 1981MNRAS.194..693L, 1991) and PKSCAT90. Cats.<VIII/16> and <VIII/15> respectively. --- S843t Total flux density at 843 MHz, in Jy number=2 This column gives the integrated flux density in Jy at 843 MHz from observations with the Molonglo Observatory Synthesis Telescope (MOST) from Jones & McAdam (1992ApJS...80..137J). The uncertainty is estimated as +/- 9 %. Jy l_S2.3G Flag for 2.3 GHz core flux density number=3 These columns give the core flux density, or upper limit, in mJy at 2.3 and 8.4 GHz. These flux densities were measured from the fringe amplitude on the single 275 km-baseline of the Parkes-Tidbinbilla Interferometer (PTI, Norris et al. 1988ApJS...67...85N). If there is source structure on the scale of the fringe spacing (100 milliarcsec at 2.3 GHz and 30 milliarcsec at 8.4 GHz) then the flux densities differ from the 'point source' flux. The cores are also expected to be variable. The combined effect is to give any uncertainty estimated at +/- 20 % in core flux. An example is Centaurus A = 1322-427 which has structure on the Parkes-Tidbinbilla baseline and a variable core. --- S2.3G Core flux density or upper limit at 2.3 GHz number=3 These columns give the core flux density, or upper limit, in mJy at 2.3 and 8.4 GHz. These flux densities were measured from the fringe amplitude on the single 275 km-baseline of the Parkes-Tidbinbilla Interferometer (PTI, Norris et al. 1988ApJS...67...85N). If there is source structure on the scale of the fringe spacing (100 milliarcsec at 2.3 GHz and 30 milliarcsec at 8.4 GHz) then the flux densities differ from the 'point source' flux. The cores are also expected to be variable. The combined effect is to give any uncertainty estimated at +/- 20 % in core flux. An example is Centaurus A = 1322-427 which has structure on the Parkes-Tidbinbilla baseline and a variable core. mJy l_S8.4G flag for 8.4 GHz core flux density number=3 These columns give the core flux density, or upper limit, in mJy at 2.3 and 8.4 GHz. These flux densities were measured from the fringe amplitude on the single 275 km-baseline of the Parkes-Tidbinbilla Interferometer (PTI, Norris et al. 1988ApJS...67...85N). If there is source structure on the scale of the fringe spacing (100 milliarcsec at 2.3 GHz and 30 milliarcsec at 8.4 GHz) then the flux densities differ from the 'point source' flux. The cores are also expected to be variable. The combined effect is to give any uncertainty estimated at +/- 20 % in core flux. An example is Centaurus A = 1322-427 which has structure on the Parkes-Tidbinbilla baseline and a variable core. --- S8.4G Core flux density or upper limit at 8.4 GHz number=3 These columns give the core flux density, or upper limit, in mJy at 2.3 and 8.4 GHz. These flux densities were measured from the fringe amplitude on the single 275 km-baseline of the Parkes-Tidbinbilla Interferometer (PTI, Norris et al. 1988ApJS...67...85N). If there is source structure on the scale of the fringe spacing (100 milliarcsec at 2.3 GHz and 30 milliarcsec at 8.4 GHz) then the flux densities differ from the 'point source' flux. The cores are also expected to be variable. The combined effect is to give any uncertainty estimated at +/- 20 % in core flux. An example is Centaurus A = 1322-427 which has structure on the Parkes-Tidbinbilla baseline and a variable core. mJy l_Sp+Index limit flag for spectral index number=4 These columns give the core spectral index (alpha, where core flux density is proportional to frequency to the power alpha, i.e., S_{nu}_ {prop.to} {nu}^{alpha}^), or upper/lower limits to core spectral index, calculated from the core flux densities at 2.3 and 8.4 GHz. These spectral index values for individual sources should be treated with caution: due to the effects of source structure on the scale of the Parkes-Tidbinbilla baseline and source variability (since the data at the two frequencies were taken months apart) the spectral index has an uncertainty estimated as +/- 0.2. --- Sp+Index Core spectral index value, or upper/lower limit number=4 These columns give the core spectral index (alpha, where core flux density is proportional to frequency to the power alpha, i.e., S_{nu}_ {prop.to} {nu}^{alpha}^), or upper/lower limits to core spectral index, calculated from the core flux densities at 2.3 and 8.4 GHz. These spectral index values for individual sources should be treated with caution: due to the effects of source structure on the scale of the Parkes-Tidbinbilla baseline and source variability (since the data at the two frequencies were taken months apart) the spectral index has an uncertainty estimated as +/- 0.2. --- RAh Right Ascension (B1950) (hour) number=5 These columns give the B1950 right ascension and declination of the radio centroid position, in degrees and in radians, from the 843 MHz MOST data (Jones & McAdam 1992ApJS...80..137J). These positions have an accuracy of 1.6" in right ascension and 2.2" cosec(dec) in declination. Note that they are not the core positions. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=5 These columns give the B1950 right ascension and declination of the radio centroid position, in degrees and in radians, from the 843 MHz MOST data (Jones & McAdam 1992ApJS...80..137J). These positions have an accuracy of 1.6" in right ascension and 2.2" cosec(dec) in declination. Note that they are not the core positions. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec Patricio Ortiz CDS 1999 Apr 07 UNKNOWN UNKNOWN "The catalogue was originally archived as R121 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_MNRAS_268_602.xml The APM galaxy survey. IV. Redshifts of rich clusters of galaxies. J/MNRAS/269/151 J/MNRAS/269/151 APM cluster redshift survey The APM galaxy survey. IV. Redshifts of rich clusters of galaxies. G B Dalton G Efstathiou S J Maddox W J Sutherland Mon. Not. R. Astron. Soc. 269 151 1994 1994MNRAS.269..151D The APM galaxy survey. IV. Redshifts of rich clusters of galaxies. G B Dalton G Efstathiou S J Maddox W J Sutherland Mon. Not. R. Astron. Soc. 273 258 1995 1995MNRAS.273..258D Clusters, galaxy Redshifts cosmology: observations galaxies: clusters: general galaxies: distances and redshifts We present redshifts for a sample of 228 clusters selected from the APM Galaxy Survey, 188 of which are new redshift determinations. Redshifts are listed for 365 galaxies, and non-cluster galaxy redshifts have been rejected from this sample using a likelihood ratio test based on the projected and apparent magnitude distributions of each cluster region. We test this technique using clusters for which redshifts have been measured for more than 10 galaxies. Our redshift sample is nearly complete and has been used in previous papers to study the three-dimensional distribution of rich clusters of galaxies. 156 of the clusters in our sample are listed in the Abell catalogue or supplement, and the remainder are new cluster identifications.
Clusters for which redshifts were found in Andernach's compilation RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec mX Characteristic magnitude number=1 Those clusters with no entries in mX and R are nearby systems which could be missed in the percolation stage of our cluster selection procedure mag R Richness number=1 Those clusters with no entries in mX and R are nearby systems which could be missed in the percolation stage of our cluster selection procedure --- z Redshift --- Abell Abell name --- Clusters observed using AUTOFIB RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec mX Characteristic magnitude number=1 Those clusters with no entries in mX and R were included in the original selection for the AUTOFIB observations and are included in the final list as nearby systems mag R Richness number=1 Those clusters with no entries in mX and R were included in the original selection for the AUTOFIB observations and are included in the final list as nearby systems --- z Redshift --- o_z Number of galaxies for which redshifts were obtained --- Abell Abell name --- Sep when Abell2 exists --- Abell2 Second Abell name --- Redshifts for galaxies in clusters observed using a single slit RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec zObs Observed redshift --- zL Maximum likelihood redshift estimate --- Proba Probability to be a cluster member % n_Proba Note on Proba number=1 * : This galaxy is rejected on the basis of the likelihood ratio test t : The likelihood function for this cluster is unstable. If the galaxy redshifts agree then this is adopted as the cluster redshift. --- z Adopted maximum likelihood redshift --- Proba2 Adopted probability of cluster membership % n_Proba2 Note on Pint number=1 * : This galaxy is rejected on the basis of the likelihood ratio test t : The likelihood function for this cluster is unstable. If the galaxy redshifts agree then this is adopted as the cluster redshift. --- Cluster redshifts obtained using the likelihood ratio test RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec mX Characteristic magnitude number=1 1: This work (AAT long-slit) 2: This work (A.N.U. 2.3m) 3: Data taken form Andernach (1991) 4: Obtained from Huchra (private communication) mag R Richness number=1 1: This work (AAT long-slit) 2: This work (A.N.U. 2.3m) 3: Data taken form Andernach (1991) 4: Obtained from Huchra (private communication) --- z Redshift --- r_z Source of the redshift --- Abell Abell name --- Sep when Abell2 exists --- Abell2 Second Abell name --- James Marcout, Patricia Bauer, Francois Ochsenbein CDS 1995 Jun 01 UNKNOWN UNKNOWN * 23-Feb-1995: Keypunched at CDS * 01-Jun-1995: Thanks to H. Andernach, errata reported in tables 2 and 4. * 02-Dec-1998: Thanks to Ivan Valtchanov (ivan@astro.bas.bg), three further typos corrected in table3. J_MNRAS_269_151.xml The structure of the Universe traced by rich clusters of galaxies J/MNRAS/269/301 J/MNRAS/269/301 Superclusters and voids The structure of the Universe traced by rich clusters of galaxies M Einasto J Einasto E Tago G B Dalton H Andernach Mon. Not. R. Astron. Soc. 269 301 1994 1994MNRAS.269..301E Clusters, galaxy galaxies: clusters: general large-scale structure of universe We study the whole-sky distribution of rich clusters of galaxies up to the distance z~0.1 and present catalogues of superclusters and cluster-defined voids. The data on clusters, superclusters and voids show the presence of the characteristic scale of 130h^-1^Mpc in the supercluster-void network, found earlier by Broadhurst et al. (1990Natur.343..726B) from a one-dimensional study. This scale has been detected in the distribution of clusters of richnesses R=0 and R>=1. We perform tests to study the influence of projection effects. The clusters that do not belong to superclusters are located in the vicinity of superclusters and form their outlying parts. We compare the distribution of ACO clusters with that of APM clusters. The APM clusters determine a smaller scale: 100h^-1^Mpc. We discuss the possible reasons for this difference.
Superclusters SC Number of the supercluster --- Nmembers Number of clusters in supercluster --- RAdeg Centre coordinates for supercluster (B1950) deg DEdeg Centre coordinates for supercluster (B1950) deg Dist Distance to the supercluster centre (from earth) (in h^-1^Mpc) Mpc Xpos Supergalactic X coordinate Mpc Ypos Supergalactic Y coordinate Mpc Zpos Supergalactic Z coordinate Mpc Length Length of the supercluster Mpc *List of supercluster members SC Supercluster number --- ZZXV Number of supercluster with common members from the catalogue by Zucca et al. (1993ApJ...407..470Z) --- ID Identification of supercluster --- ACO Abell-ACO (Cat. <VII/110>) number of member cluster --- n_ACO Membership flag number=1 "e" only estimated redshift available "x" X-ray cluster "?" background cluster ? (Dalton et al. (1994), Cat. <J/MNRAS/269/151>) --- Parameters of voids VoisNo Number of void --- RAdeg Coordinates of void centre (B1950) deg DEdeg Coordinates of void centre (B1950) deg Dist Distance to the void centre (in h^-1^Mpc) Mpc Diam Minos axis of void (in h^-1^Mpc) Mpc SCL Numbers of superclusters at void walls --- Com Comments --- Patricia Bauer CDS 1996 Oct 22 We thank H. Andernach <heinz@cuevano.ugto.mx> for providing an electronic copy of the tables (#A191 in his list) UNKNOWN UNKNOWN * 09-Dec-1996: a new version of Table3 was provided by H. Andernach (see the Note on table3 above). J_MNRAS_269_301.xml Expectancy of large pulsar glitches: a comparison of models with the observed glitch sample J/MNRAS/269/849 J/MNRAS/269/849 Pulsar glitches Expectancy of large pulsar glitches: a comparison of models with the observed glitch sample M A Alpar A Baykal Mon. Not. R. Astron. Soc. 269 849 1994 1994MNRAS.269..849A Pulsars MHD pulsars: general stars: interiors stars: rotation We study the expectancy of large glitches ({Delta}{Omega}/{Omega}>10^-7) from a sample of 430 pulsars other than the Vela pulsar. The pulsars in this sample have exhibited 19 large glitches. We assume that all pulsars experience such glitches, with rates that depend on the pulsar's rotation rate omega and spin-down rate omega, and on the glitch model. We use the core-quake model, and two variants of the superfluid vortex unpinning model, and choose model parameters such that the observed number of glitches is matched by the theoretically expected number. Among the models investigated, one of the superfluid vortex unpinning models gives good agreement with the observed distribution of glitches and with the parameter values deduced for the Vela pulsar glitches.
Time-spans of glitch-monitoring observations PSR PSR name --- t Time-spans d Ref References number=1 References: A : Ashworth & Lyne (1981MNRAS.195..517A) B : Backus et al. (1982ApJ...255L..63B) D : Downs G. S. (1982, private communication) G : Gullahom & Rankin (1978AJ.....83.1219G) H : Helfand et al. (1980ApJ...237..206H) M : Manchester et al. (1983MNRAS.202..269M) N : Newton et al. (1981, MNRAS 194, 841) (D) : Dewey et al. (1988ApJ...332..762D) (J) : Jones & Lyne (1988MNRAS.232..473J) T : Taylor & Dewey (1988ApJ...332..770T) C : McConnell et al. (1991MNRAS.249..654M) (G) : Gouiffes et al. (1992ApJ...394..581G) (JM): Johnston et al. (1992ApJ...387L..37J) K : Kaspi et al. (1992ApJ...399L.155K) S : Siegman, Manchester & Durdin (1993MNRAS.262..449S) J : Johnston et al. (1995A&A...293..795J) L : Lyne (private communication). --- James Marcout, Patricia Bauer CDS 1996 Oct 01 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_269_849.xml Globular clusters in the Magellanic Clouds - II. IR-array photometry for 12 globular clusters and contributions to the integrated cluster light. J/MNRAS/272/391 J/MNRAS/272/391 Globular clusters in the Magellanic Clouds Globular clusters in the Magellanic Clouds - II. IR-array photometry for 12 globular clusters and contributions to the integrated cluster light. F R Ferraro F Fusi Pecci V Testa L Greggio C E Corsi R Buonanno D M Terndrup H Zinnecker Mon. Not. R. Astron. Soc. 272 391 1995 1995MNRAS.272..391F globular clusters: general Hertzsprung-Russell (HR diagram) infrared: stars Magellanic Clouds stars: AGB and post-AGB stars: evolution We report JHK results of observations of 12 globular clusters in the Large Magellanic Cloud (LMC), and present colour-magnitude diagrams down to K=16 (corresponding to absolute K~-2.6) for ~450 stars in these clusters.
IR photometric data from literature Cluster Cluster name --- Kmag Integrated K magnitude mag Aperture Diaphragm aperture used for integrated photometry from Persson S.E. et al. 1983 number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. arcsec V-K Integrated intrinsic V-K colour from Persson S.E. et al. 1983 number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. mag J-K Integrated intrinsic J-K colour from Persson S.E. et al. 1983 number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. mag H-K Integrated intrinsic H-K colour from Persson S.E. et al. 1983 number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. mag B-V B-V colour from van den Berg S. 1981 number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. mag r_B-V Reference for B-V number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. --- e(B-V) B-V estimate mag r_e(B-V) Reference for B-V estimate number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. --- SWB Type (ref.(1) in note (1)) --- r_SWB Reference for SWB-type number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. --- s s-parameter as defined in Elson and Fall 85 number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. --- r_s Reference for the s-parameter number=1 (1) Searle L., Wilkinson A., Bagnuolo W.G., 1980 ApJ, 239, 803; (2) Elson R.A.W. and Fall S.M. 1985 ApJ, 299, 211; (3) Persson S.E. et al. 1983 ApJ, 266, 105; (4) Freeman K. et al. 1983 ApJ, 272, 488; (5) Meurer G.R. et al. 1990 AJ, 99, 1124; (6) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (7) Bica E. et al. 1986 A&A, 156, 261; (8) Schommer et al. 1984 ApJ, 285, L53; (9) Chiosi C. and Pigatto L. 1986 ApJ, 308, 1; (10) Mould J.R. et al. 1986 ApJ, 309, 39; (11) Mould J.R. and Da Costa G.S. 1988, in Blanco V.M., Phillips M.M., eds, ASP Conf. Ser. Vol. 1, Progress and Opportunities in Southern Hemisphere Optical Astronomy. Astron. Soc. Pac., San Francisco, p.197; (12) Burstein D. and Heiles C. 1982, AJ, 87, 1165; (13) Westerlund B.E. 1990 A&AR, 2, 29; (14) Dottori H. et al. 1987 Rev. Mex. Astron. Astrofis., 14, 183; (15) Vallenari A. et al. 1992 AJ, 104, 1100; (16) van den Berg S. 1981, A&AS, 46, 79; (17) Mateo M. 1987 ApJ, 323, L41; (18) Bica E. et al. 1991 ApJ, 381, L51. --- Magnitudes, colours and positions for the programme stars in each cluster Cluster Cluster name --- Star Star number --- Kmag K magnitude mag J-K J-K colour index mag H-K H-K colour index mag V-K V-K colour index mag B-V B-V colour index mag Xpos X star position at a scale of 0.92 arcsec/pix pix Ypos Y star position at a scale of 0.92 arcsec/pix pix Cross-identifications and comparisons with the literature Cluster Cluster name --- r_Star Reference star number number=1 MA=Mould J.R. and Aaronson M. 1980, 1982 or Aaronson M. and Mould J.R. 1982, 1985 (2); LE= Lloyd-Evans T.L.E. 1980 MNRAS, 193, 87; W= Walker 1971 ApJ, 167, 1. --- Star Star number --- MAsource Source from Mould and Aaronson 1980, 1982 or Aaronson and Mould 1982, 1985 (MA) number=2 (1) Mould J.R. and Aaronson M. 1980 ApJ, 240, 464; (2) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (3) Mould J.R. and Aaronson M. 1982 ApJ, 263, 629; (4) Aaronson M. and Mould J.R. 1985 ApJ, 288, 551. --- MAKmag K magnitude from MA mag MAJ-K J-K colour from MA mag MAH-K H-K colour from MA mag FMB Source number from Frogel et al. 1990 number=2 (1) Mould J.R. and Aaronson M. 1980 ApJ, 240, 464; (2) Aaronson M. and Mould J.R. 1982 ApJS, 48, 161; (3) Mould J.R. and Aaronson M. 1982 ApJ, 263, 629; (4) Aaronson M. and Mould J.R. 1985 ApJ, 288, 551. --- FMBKmag K magnitude from FMB mag FMBJ-K J-K colour from FMB mag FMBH-K H-K colour from FMB mag TP Source number from this paper --- TPKmag K magnitude from this paper mag TPJ-K J-K colour from this paper mag TPH-K H-K colour from this paper mag Observed and normalized numbers of AGB and RGB stars Cluster Cluster name --- AGB Number of stars in the AGB (Asymptotic Giant Branch) phase of evolution --- RGB Number of stars in the RGB (Red Giant Branch) phase of evolution --- BolMag Bolometric magnitude mag Lum Cluster luminosity in units of solar luminosity solLum N4 Number of giants within the range 10<K<14.3, normalized to the luminosity of each cluster in units of 10^4^L_sun_. --- N*(AGB) Number of AGB stars normalized to 10^4^L_sun_ --- N*(RGB) Number of RGB stars normalized to 10^4^L_sun_ --- s Cluster type --- AGB and RGB contributions to the luminosity of the cluster Cluster Cluster name --- LumK(AGB) Contribution of AGB stars to the cluster luminosity in K, as a fraction of total luminosity --- LumK(RGB) Contribution of RGB stars to the cluster luminosity in K, as a fraction of the total luminosity --- BolMag Bolometric magnitude mag Bol(RGB) Contribution of RGB stars to the cluster bolometric luminosity, as a fraction of the total luminosity --- s s-parameter as defined in Elson R.A.W. and Fall S.M. 1985, ApJ, 299, 211. --- Theoretical quantities Ref Literature reference number=1 References: SGR= Sweigart A.V. et al. 1989 ApJS, 69, 911 and Sweigart A.V. et al. 1990, ApJ, 364, 527; Al93C= Alongi M. et al. 1993 A&AS, 97, 851, standard models; Al93O= Alongi M. et al. 1993 A&AS, 97, 851, overshooting models. --- log(Age) Age of RGB stars yr Bol(RGB) Predicted contribution of RGB stars to the cluster bolometric luminosity, as a fraction of the total luminosity --- Comparisons between observed and computed integrated colours and magnitudes Cluster Cluster name --- Aperture Diaphragm aperture arcsec Kmag1 K magnitude in literature (see table1) mag J-K1 J-K colour index in literature (see table1) mag Kmag2 K magnitude obtained by adding the contribution of all the stars detected in this survey mag J-K2 J-K colour index obtained by adding the contribution of all the stars detected in this survey mag AGB and RGB contributions to the integrated colours Cluster Cluster name --- J-K Integrated J-B colour obtained by adding the contribution of all the stars detected in this survey mag J-K(AGB) J-K colour obtained after the deletion of the AGB stars mag J-K(RGB) J-K colour obtained after the deletion of the RGB stars mag V-K Integrated V-K colour from table1 mag V-K(AGB) Integrated V-K colour obtained after the deletion of the AGB stars mag V-K(RGB) V-K colour obtained after the deletion of the RGB stars mag B-V Integrated B-V colour mag B-V+ B-V colour after the deletion of the red stars (AGB+RGB) mag James Marcout, Simona Mei CDS 1995 Apr 05 UNKNOWN UNKNOWN Keypunched at CDS J_MNRAS_272_391.xml The 5C13 deep radio survey (16h, +42) J/MNRAS/272/699 J/MNRAS/272/699 The 5C13 deep radio survey The 5C13 deep radio survey (16h, +42) C R Benn Mon. Not. R. Astron. Soc. 272 699 1995 1995MNRAS.272..699B radio continuum: general surveys A deep 0.4-GHz survey of a 4deg-diameter region in Hercules is reported. 232 sources brighter than 9.5 mJy were detected. In a simultaneous 1.4-GHz survey of the concentric area 1deg in diameter, 45 sources brighter than 1.7 mJy were detected. The differential 0.4-GHz radio source count is presented; it is in good agreement with that from other 5C surveys. This survey brings to 3220 the number of 0.4-GHz sources catalogued by the published 5C surveys.
The 5C13 catalogue 5C13 5C13 serial number --- RAh Right ascension (1950) number=1 measured at 0.4 GHz or, if detected at higher frequency, at 1.4 GHz h RAm Right ascension (1950) number=1 measured at 0.4 GHz or, if detected at higher frequency, at 1.4 GHz min RAs Right ascension (1950) number=1 measured at 0.4 GHz or, if detected at higher frequency, at 1.4 GHz s DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec e_RA rms uncertainty in measured right ascension arcsec S0.4 Peak 0.4-GHz flux density mJy e_S0.4 rms uncertainty on flux density mJy P0.4 Envelope attenuation at 0.4-GHz number=2 S0.4 must be multiplied by this factor to recover the apparent flux density S'0.4 with which the source appears on the synthesized map, and hence the signal-to-noise ratio --- S1.4 Peak 1.4-GHz flux density mJy e_S1.4 rms uncertainty on flux density mJy P1.4 Envelope attenuation at 1.4-GHz number=2 S0.4 must be multiplied by this factor to recover the apparent flux density S'0.4 with which the source appears on the synthesized map, and hence the signal-to-noise ratio --- Alpha Radio spectral index {alpha} (0.4, 1.4 GHz) --- Notes Notes --- 5C13 0.4-GHz source counts S0.4(1) Peak 0.4-GHz lower limit for the flux density range mJy S0.4(2) Peak 0.4-GHz upper limit for the flux density range mJy m1 Number of sources detected in the given flux density range before polar-diagram correction --- m2 Number of sources detected in the given flux density range after polar-diagram correction --- DelN Source density 10+5sr-1 5C13DelN/No 5C13 Source density number=3 Normalized to Euclidean integral count 750(S/Jy)^-1.5^/sr --- e_5C13DelN/No Error on source density --- 5CDelN/No Mean source density (3) for the published 5C surveys number=1 Benn and Wall 1995 --- e_5CDelN/No Error on source density --- B3DelN/No Mean source density (3) for the B3 survey number=2 Grueff 1988 --- e_B3DelN/No Error on source density --- James Marcout, Simona Mei CDS 1995 Aug 16 UNKNOWN UNKNOWN #A022 in H. Andernach's list; Completed at CDS J_MNRAS_272_699.xml Multicolour CCD surface photometry for E and S0 galaxies in 10 clusters J/MNRAS/273/1097 J/MNRAS/273/1097 CCD photometry for E and S0 galaxies Multicolour CCD surface photometry for E and S0 galaxies in 10 clusters I Jorgensen M Franx P Kjaergaard MNRAS 273 1097 1995 1995MNRAS.273.1097J Clusters, galaxy Galaxies, photometry CCD surface photometry for 232 E and S0 galaxies is presented. The galaxies are observed in Gunn r and Johnson B, or Gunn r and g. For 48 of the galaxies also surface photometry in Johnson U is presented. Aperture magnitudes in Gunn v are derived for half of the galaxies. Galaxies in the following clusters have been observed: Abell 194, Abell 539, Abell 3381, Abell 3574, Abell S639, Abell S753, HydraI (Abell 1060), DC2345-28, Doradus, and Grm15. This catalog include the global parameters for the galaxies: effective radius, mean surface brightness, the characteristic radius r_n, colour, colour gradient, ellipticity, c4, <c4>, and <c6>. The derivation of the effective parameters and of r_n takes the seeing into account. Seeing corrected values of the effective parameters and r_n are given for 147 E and S0 galaxies in the Coma cluster. This catalog also includes colours, colour gradients, ellipticity, c4, <c4>, and <c6> for the galaxies in the Coma cluster. This is an slightly updated version of data published in Jorgensen et al. (A&AS, 95, 489 (1992)) and Jorgensen & Franx (ApJ, 433, 553 (1994)). Colours and ellipticities are derived for the values effective radii in Gunn r where the seeing has been taken into account.
Global parameters in Gunn r Global parameters in Gunn r for galaxies in the Coma cluster Cluster Cluster name --- Galaxy Galaxy name --- lre_GR log10(r_e in arcsec) r_e is the effective equivalent radius in arcsec derived from a fit to an r**1/4 growth curve --- e_lre_GR Uncertainty on lre_GR --- mue_GR Mean surface brightness within r_e mag/arcsec2 e_mue_GR Uncertainty on mue_GR mag/arcsec2 lrn_GR log10(r_n in arcsec) r_n is the equivalent radius within which the mean surface brightness in Gunn r is 19.60mag/arcsec2 --- n_lrn_GR Flag for seeing correction of lrn_GR 0 : seeing correction on log_rn smaller than 0.05 5 : seeing correction on log_rn 0.05-0.1 10 : seeing correction on log_rn 0.1-0.2 --- eps_re Ellipticity at r_e --- eps_2185 Ellipticity at local surface brightness 21.85mag/arcsec2 --- c4 Average extremum of c4 c4 is the average of three values of the coefficient for the cos(4*theta) term of the Fourier expansion of the deviations of the isophotes from perfect ellipses. The average is taken around the minimum or maximum of the radial profile of the coefficient. In case of no well-defined extremum, the average is taken at r_e. --- u_c4 Uncertainty flag on c4 : Uncertainty smaller than 0.01 2 : Uncertainty 0.01-0.02 1 : Uncertainty larger than 0.02 --- <c4> Intensity weighted mean c4 <c4> is the intensity weighted mean of the coefficient for the cos(4*theta) term of the Fourier expansion of the deviations of the isophotes from perfect ellipses (Jorgensen & Franx ApJ, 433, 553 (1994)). --- u_<c4> Uncertainty flag on <c4> --- <c6> Intensity weighted mean c6 <c6> is the intensity weighted mean of the coefficient for the cos(6*theta) term of the Fourier expansion of the deviations of the isophotes from perfect ellipses (Jorgensen & Franx ApJ, 433, 553 (1994)). --- u_<c6> Uncertainty flag on <c6> --- c4_class Classification of c4 radial profile Classification of the radial profile of the coefficient for the cos(4*theta) term of the Fourier expansion of the deviations of the isophotes from perfect ellipses. reg/d : regular, c4 dominating reg/nd: regular, c4 not dominating irr/d : irregular, c4 dominating irr/nd: irregular, c4 not dominating --- Global parameters in Gunn g, Johnson B and U (A194 & DC2345-28, Other) Cluster Cluster name --- Galaxy Galaxy name --- lre_GG log10(r_e in arcsec) in Gunn g r_e is the effective equivalent radius in arcsec derived from a fit to an r**1/4 growth curve --- e_lre_GG Uncertainty on lre_GG --- mue_GG Mean surface brightness within r_e in Gunn g mag/arcsec2 e_mue_GG Uncertainty on mue_GG mag/arcsec2 lrn_GG log10(r_n in arcsec) in Gunn g r_n is the equivalent radius within which the mean surface brightness in Gunn g is 20.05mag/arcsec2, in Johnson B is 20.75mag/arcsec2, and in Johnons U is 21.25mag/arcsec2 --- n_lrn_GG Flag for seeing correction of lrn_GG -- : seeing correction on log_rn smaller than 0.05 5 : seeing correction on log_rn 0.05-0.1 10 : seeing correction on log_rn 0.1-0.2 --- lre_JB log10(r_e in arcsec) in Johnson B --- e_lre_JB Uncertainty on lre_JB --- mue_JB Mean surface brightness within r_e in Johnson B mag/arcsec2 e_mue_JB Uncertainty on mue_JB mag/arcsec2 lrn_JB log10(r_n in arcsec) in Johnson B --- n_lrn_JB Flag for seeing correction of lrn_JB --- lre_JU log10(r_e in arcsec) in Johnson U --- e_lre_JU Uncertainty on lre_JU --- mue_JU Mean surface brightness within r_e in Johnson U mag/arcsec2 e_mue_JU Uncertainty on mue_JU mag/arcsec2 lrn_JU log10(r_n in arcsec) in Johnson U --- n_lrn_JU Flag for seeing correction of lrn_JU --- Colours, colour gradients (A194 & DC2345-28, Other) Cluster Cluster name --- Galaxy Galaxy name --- g_r Colour GG - GR within r_e in Gunn r --- v_r Colour GV - GR within r_e in Gunn r --- B_r Colour JB - GR within r_e in Gunn r --- g_r Colour JU - GR within r_e in Gunn r --- grad_Br Colour gradient in JB_GR The colour gradients are derived from linear fits to the colour versus the logarithm of the radius. --- e_grad_Br Uncertainty on grad_Br --- q_grad_Br Quality flag on grad_Br 1: The colour gradients are derived from the radius interval where the uncertainty on JB-GR is below 0.025mag and the uncertainty on JU-GR is below 0.035mag. 2: The colour gradients are derived from the radius interval where the uncertainty on JB-GR is below 0.05mag and the uncertainty on JU-GR is below 0.07mag. --- grad_Ur Colour gradient in JU_GR --- e_grad_Ur Uncertainty on grad_Ur --- q_grad_Ur Quality flag on grad_Ur --- Global parameters in Johnson B, colours, colour gradients (A3574 & S753) Global parameters in Johnson B, colours, colour gradients (Coma) Cluster Cluster name --- Galaxy Galaxy name --- lre_JB log10(r_e in arcsec) in Johnson B r_e is the effective equivalent radius in arcsec derived from a fit to an r**1/4 growth curve --- e_lre_JB Uncertainty on lre_JB --- mue_JB Mean surface brightness within r_e in Johnson B mag/arcsec2 e_mue_JB Uncertainty on mue_JB mag/arcsec2 lrn_JB log10(r_n in arcsec) in Johnson B r_n is the equivalent radius within which the mean surface brightness in Johnson B is 20.75mag/arcsec2. --- n_lrn_JB Flag for seeing correction of lrn_JB : seeing correction on log_rn smaller than 0.05 5 : seeing correction on log_rn 0.05-0.1 10 : seeing correction on log_rn 0.1-0.2 --- v_r Colour GV - GR within r_e in Gunn r --- B_r Colour JB - GR within r_e in Gunn r --- grad_Br Colour gradient in JB_GR The colour gradients are derived from linear fits to the colour versus the logarithm of the radius. --- e_grad_Br Uncertainty on grad_Br --- q_grad_Br Quality flag on grad_Br 1: The colour gradients are derived from the radius interval where the uncertainty on JB-GR is below 0.025mag. 2: The colour gradients are derived from the radius interval where the uncertainty on JB-GR is below 0.05mag. -------------------------------------------------------------------------------- z Byte-by-byte Description of file: tableA5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Cluster Cluster name 11- 19 A9 --- Galaxy Galaxy name 23- 27 F5.2 --- lre_GG *log10(r_e in arcsec) in Gunn g 31- 34 F4.2 --- e_lre_GG Uncertainty on lre_GG 37- 41 F5.2 mag/arcsec2 mue_GG Mean surface brightness within r_e in Gunn g 45- 48 F4.2 mag/arcsec2 e_mue_GG Uncertainty on mue_GG 51- 55 F5.2 --- lrn_GG *log10(r_n in arcsec) in Gunn g 58- 59 I2 --- n_lrn_GG *Flag for seeing correction of lrn_GG 62- 66 F5.2 --- g_r Colour GG - GR within r_e in Gunn r 69- 73 F5.2 --- v_r ?Colour GV - GR within r_e in Gunn r --- Global parameters in Gunn g, colours (A539, A3381, S639, Hydra) Cluster Cluster name --- Galaxy Galaxy name --- lre_GG log10(r_e in arcsec) in Gunn g r_e is the effective equivalent radius in arcsec derived from a fit to an r**1/4 growth curve --- e_lre_GG Uncertainty on lre_GG --- mue_GG Mean surface brightness within r_e in Gunn g mag/arcsec2 e_mue_GG Uncertainty on mue_GG mag/arcsec2 lrn_GG log10(r_n in arcsec) in Gunn g r_n is the equivalent radius within which the mean surface brightness in Gunn g is 20.05mag/arcsec2. --- n_lrn_GG Flag for seeing correction of lrn_GG -- : seeing correction on log_rn smaller than 0.05 5 : seeing correction on log_rn 0.05-0.1 10 : seeing correction on log_rn 0.1-0.2 --- g_r Colour GG - GR within r_e in Gunn r --- Inger Jorgensen McDonald Observatory, Austin, Texas 1995 June 13 J_MNRAS_273_1097.xml A faint galaxy redshift survey to B = 24. J/MNRAS/273/157 J/MNRAS/273/157 A faint galaxy survey to B = 24. A faint galaxy redshift survey to B = 24. K Glazebrook R Ellis M Colless T Broadhurst J Allington-Smith N Tanvir Mon. Not. R. Astron. Soc. 273 157 1995 1995MNRAS.273..157G Galaxies, photometry Redshifts Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5<B<24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z>1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.
Table 3 of publication Field Field number number=1 the numeric values correspond to fields: 03.31 = 03z3_A (B limit for 70% completeness: 24.0mag) 10.21 = 10z2_A (B limit for 70% completeness: 24.0mag) 10.22 = 10z2_B (B limit for 70% completeness: 24.0mag) 10.23 = 10HST1 (B limit for 70% completeness: 24.0mag, and B>22.5) 13.21 = 13z2_A (B limit for 70% completeness: 23.3mag) 13.22 = 13HST1 (B limit for 70% completeness: 23.5mag, and B>22.5) 22.31 = 22z3_A (B limit for 70% completeness: 23.0mag) --- Slit The object's LEXT box --- ID The object's unique ID number [GEC95] number=2 The object's unique ID number (designated [GEC95] in SIMBAD) is of the form ff.nnn , where ff = RA field (03, 10 etc.) and nnn = ID number in photometric catalogue (e.g. 10.288 is #288 in 10z2_Bcdd catalog) --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Bmag Magnitude in B, zero when no data mag e_Bmag Mean error on Bmag mag Rmag Magnitude in R, zero when no data mag n_Rmag 'f' if not detected in R band --- e_Rmag Mean error on Rmag mag Imag Magnitude in I, zero when no data mag n_Imag 'f' if not detected in I band --- e_Imag Mean error on Imag mag z Redshift number=3 the value 9.999 indicates UnIDitenfied, and a value of 0.000 indicates a star. --- Ty Spectrum type number=4 The spectrum type is A = Absorption line galaxy E = Emission line galaxy Q = QSO --- EW Equivalent width of [OII] number=5 Equivalent width of [OII] line (3727Angstroems at rest): when EW=0 and e_EW>0 then e_EW represents an upper limit; when EW=0 and e_EW=0 then no value is known. 0.1nm e_EW Mean error or upper limit on EW number=5 Equivalent width of [OII] line (3727Angstroems at rest): when EW=0 and e_EW>0 then e_EW represents an upper limit; when EW=0 and e_EW=0 then no value is known. 0.1nm Q Quality criterium number=6 the values of Q are: Q = 1 : certain Q = 2 : uncertain Q = 3 : no identification Q = 4 : dud, missing --- Comments found in spectrum etc. number=7 The following symbols are used: + = emission ; - = absorption; Missing? = no apparent signal; Weak = barely detected continuum; Featureless = well-detected continuum, but no real features --- Francois Ochsenbein CDS 1995 Aug 18 Karl Glazebrook <kgb@ast.cam.ac.uk> <http://www.ast.cam.ac.uk/~kgb/papers.html> UNKNOWN UNKNOWN Nomenclature Notes: [GEC95] followed by the contents of the ID column of catalog is the acronym used in SIMBAD to designate the galaxies of this publication. J_MNRAS_273_157.xml Multifrequency flux density measurements of 280 pulsars. J/MNRAS/273/411 J/MNRAS/273/411 Multifrequency fluxes of 280 pulsars Multifrequency flux density measurements of 280 pulsars. D R Lorimer J A Yates A G Lyne D M Gould Mon. Not. R. Astron. Soc. 273 411 1995 1995MNRAS.273..411L VII/156 : Catalog of pulsars (Taylor+, 1993) http://www.mpifr-bonn.mpg.de/pulsar : MPIfR pulsar group Pulsars Radio sources pulsars: general radio continuum: stars Table3 contains the flux density measurements of pulsars made at radio frequencies centred around 408, 606, 925, 1408 and 1606MHz using the 76-m Lowell telescope at Jodrell Bank. The observations have been made over a period of more than 3 years and concern 280 pulsars.
Fluxes for the 280 pulsars PSRB Name of pulsar as in Taylor cat. <VII/156> --- W50 Pulse width at 50% of pulse peak the pulse widths are taken mainly from the 408MHz profile data. ms W10 Pulse width at 10% of pulse peak ms l_S408 Limit flag on S408 --- S408 Flux density at 408MHz mJy e_S408 Mean error on S408 mJy l_S606 Limit flag on S606 --- S606 Flux density at 606MHz mJy e_S606 Mean error on S606 mJy l_S925 Limit flag on S925 --- S925 Flux density at 925MHz mJy e_S925 Mean error on S925 mJy l_S1408 Limit flag on S1408 --- S1408 Flux density at 1408MHz mJy e_S1408 Mean error on S1408 mJy l_S1606 Limit flag on S1606 --- S1606 Flux density at 1606MHz mJy e_S1606 Mean error on S1606 mJy l_SI Limit flag on SI --- SI Spectral index (F(nu) prop.to. (nu)**(SI)) --- e_SI Limit flag on SI --- spectra.ps Postscript spectra (completed Figure 1) Francois Ochsenbein CDS 1998 Jan 26 The table was kindly supplied by Dunc Lorimer <dunc@mpifr-bonn.mpg.de> in January 1998. J_MNRAS_273_411.xml The Edinburgh-Durham Southern Galaxy Catalogue - VII. The Edinburgh-Milano cluster redshift survey J/MNRAS/274/1071 J/MNRAS/274/1071 Edinburgh-Milano cluster redshift survey The Edinburgh-Durham Southern Galaxy Catalogue - VII. The Edinburgh-Milano cluster redshift survey C A Collins L Guzzo R C Nichol S L Lumsden Mon. Not. R. Astron. Soc. 274 1071 1995 1995MNRAS.274.1071C VII/175 : Edingburgh-Durham Cluster Catalogue (Lumdsen+ 1992) Clusters, galaxy Redshifts catalogs cosmology: observations galaxies: clusters: general galaxies: distances and redshifts large-scale structure of universe surveys In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R>=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.
Results for galaxies in the survey with two independent observations either at the ESO 3.6-m and 2.2-m telescopes or at the AAT. EDCC Edingburgh-Durham Cluster Catalogue (EDCC, Cat <VII/175>) cluster identification name --- RAh Right ascension (B1950) h RAm Right ascension (B1950) min RAs Right ascension (B1950) s DE- Declination sign --- DEd Declination (B1950) deg DEm Declination (B1950) arcmin DEs Declination (B1950) arcsec bj Approximate (+/-0.25mag) apparent magnitude of the galaxy in the photographic b, band from the EDSGC mag cz1 Radial velocity determined form Tel1 observations km/s Tel1 Telescope (ESO 3.6m, ESO 2.2m or ATT) --- cz2 Radial velocity determined form Tel2 observations km/s Tel2 Telescope (ESO 3.6m, ESO 2.2m or ATT) --- HV Heliocentric velocity km/s The galaxies observed in the EM cluster redshift survey ESO and AAT EDDC EDCC cluster identification name --- RAh Right ascension (B1950) (see note 1) h RAm Right ascension (B1950) (see note 1) min RAs Right ascension (B1950) (see note 1) s DE- Declination sign --- DEd Declination (B1950) (see note 1) deg DEm Declination (B1950) (see note 1) arcmin DEs Declination (B1950) (see note 1) arcsec bj Approximate (+/-0.25mag) apparent magnitude of the galaxy in the photographic b, band from the EDSGC. mag cz Heliocentric velocity of each galaxy km/s e_cz Internal redshift error from the cross-correlation routine, described in Section 4.2. km/s Note Note on observations number=1 E: ESO observation A: AAT observation AC: A larger than normal error in the coordinates and magnitude. This is the case for galaxies which are not detected in the EDSGC, e.g. objects merged with other object images in the digitization process. NC: Two galaxies in E178, three in E261, two in E424 and three in E473 do not have a certain identification in our logfiles We prefer therefore not to list any coordinate and magnitude which would be too approximate, although we give the redshift and the information that the object belongs to that cluster. --- The clusters observed in the EM redshift survey EDCC EDCC cluster identification name --- RAh Right ascension (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. (1992MNRAS.258....1L, Cat. <VII/175>). h RAm Right ascension (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. (1992MNRAS.258....1L, Cat. <VII/175>). min RAs Right ascension (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. (1992MNRAS.258....1L, Cat. <VII/175>). s DE- Declination sign --- DEd Declination (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. (1992MNRAS.258....1L, Cat. <VII/175>). deg DEm Declination (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. (1992MNRAS.258....1L, Cat. <VII/175>). arcmin DEs Declination (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. (1992MNRAS.258....1L, Cat. <VII/175>). arcsec Ntot Total number of redshifts taken for each cluster (listed in Table 3) --- Nclus Number of cluster members determined from the deprojection algorithm described in Sect. 5.1 --- cz Mean heliocentric redshift of the galaxy members in each cluster km/s e_cz 1 sigma errors on the mean redshift of each cluster km/s sigma Radial velocity dispersions for clusters with N cluster =>6 km/s E_sigma Error in sigma (upper limit) km/s e_sigma Error in sigma (lower limit) km/s Note 'p' indicates that the cluster has been classified as a projection effect (see Sect. 5.1) --- *List of selected clusters EDCC EDCC cluster identification name --- RAh Right ascension (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. 1992MNRAS.258....1L, Cat. <VII/175> h RAm Right ascension (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. 1992MNRAS.258....1L, Cat. <VII/175> min RAs Right ascension (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. 1992MNRAS.258....1L, Cat. <VII/175> s DE- Declination sign --- DEd Declination (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. 1992MNRAS.258....1L, Cat. <VII/175> deg DEm Declination (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. 1992MNRAS.258....1L, Cat. <VII/175> arcmin DEs Declination (B1950) number=1 Equatorial coordinates of the cluster centroid, taken from Lumsden et al. 1992MNRAS.258....1L, Cat. <VII/175> arcsec R1 Number of galaxy members between the magnitudes m_3_ and m_3_+2 calculated using an Abell radius of 1h^-1^Mpc --- m10 Magnitude of the 10th brightest galaxy, after background correction, within the 1h^-1^Mpc radius mag RAbell Angular 'reduced Abell radius' calculated using the equivalent of Abell's m_10_ distance estimate --- PA Position angle of the cluster as defined in Martin et al. (1995MNRAS.274..623M) deg Eps [0/1] Eccentricity of the clusters, defined and used in Martin et al. (1995MNRAS.274..623M). --- cz Radial velocity of the cluster km/s n_cz Number of galaxies used to determine cz number=2 For the EM clusters, this is just N cluster (number of cluster members determined from the deprojection algorithm) --- Ref Source of the cluster radial velocity number=3 EM : this study Broadbent 1992 (priv. comm.) Ciardullo et al. (1985ApJ...293...69C) Dalton et al. (1994MNRAS.269..151D, Cat. <J/MNRAS/269/151>) Huchra et al. (1992, Cat. <VII/193>) Huchra (priv. comm.) Loveday (19911, PhD thesis, Univ. Cambridge) Muriel et al. (1990AJ....100..339M) Muriel et al. (1991AJ....101.1997M) Nicholson (1991, PhD thesis, Univ. Edinburgh) Olowin et al. (1988A&AS...73..125O) Peacock (priv. comm.) Peterson et al. (1986MNRAS.221..233P) Postman et al. (1992ApJ...384..404P, Cat. <J/ApJ/384/404>) Teague et al. (1990ApJS...72..715T) --- James Marcout, Patricia Bauer CDS 1997 Jan 14 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_274_1071.xml The ROSAT Wide Field Camera all-sky survey of extreme-ultraviolet sources - II. The 2RE Source Catalogue J/MNRAS/274/1165 J/MNRAS/274/1165 The 2RE Source Catalogue The ROSAT Wide Field Camera all-sky survey of extreme-ultraviolet sources - II. The 2RE Source Catalogue J P Pye P A McGale D J Allan C R Barber D Bertram M Denby C G Page M J Ricketts B C Stewart R G West Mon. Not. R. Astron. Soc. 274 1165 1995 1995MNRAS.274.1165P J/MNRAS/260/77 : the ROSAT-WFC Bright Source Catalogue (Pounds et al. 1993) J/A+AS/114/465 : the ROSAT XUV Pointed Phase Src. Cat. (Kreysing et al. 1995) II/203 : Second Extreme Ultra-Violet Explorer Catalog (1996) IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges et al. 1996) ftp://ledas-ftp.star.le.ac.uk/rosat/2re/cat : the original file X-ray sources catalogs space vehicles stars: late-type ultraviolet: general white dwarfs X-rays: general During 1990-1991 the Wide Field Camera (WFC) on the ROSAT satellite performed the first all-sky survey at EUV wavelengths. The survey was conducted in two 'colours' using broad-band filters to define wavebands covering the ranges 60-140A and 112-200A. It was fully imaging, with effective spatial resolution of about 3arcmin FWHM, and point source location accuracy of typically better than 1 arcmin. From an initial analysis, Pounds et al. published the WFC Bright Source Catalogue (BSC) of 383 sources. In this paper we report results from reprocessing of the complete survey database; the resulting list of sources is the '2RE' Catalogue. It contains 479 sources, of which 387 are detected in both survey wavebands, a significant advance on the BSC (80 per cent versus 60 per cent). Improvements over the original BSC include: (i) better rejection of poor aspect periods, and smaller random errors in the aspect reconstruction; (ii) improved background screening; (iii) improved methods for source detection; (iv) inclusion of a time-variability test for each source; (v) more extensive investigation of the survey sensitivity. We define the catalogue selection criteria, and present the catalogue contents in terms of tables and sky maps. We also discuss the sky coverage, source number-flux relations, optical identifications and source variability.
ROSAT
The 2RE catalogue, Table 2 of paper 2RE designation, based on the J2000 position. --- note indicates a note in file notes.txt --- RAh Right Ascension J2000 (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec ErrPos Position error, 90% confidence radius, due to counting statistics only. arcsec S1 S1-band count rate number=1 The bands are S1 90-206eV ( 60-140 Angstroems), mean 125eV (100A) S2 62-110eV (110-200 Angstroems), mean 90eV (140A) ct/s e_S1 1 sigma error on S1-band count rate ct/s S2 S2-band count rate number=1 The bands are S1 90-206eV ( 60-140 Angstroems), mean 125eV (100A) S2 62-110eV (110-200 Angstroems), mean 90eV (140A) ct/s e_S2 1 sigma error on S2-band count rate ct/s Sig1 S1-band detection significance number=2 see section 3.5 of the paper for an accurate definition of the acceptance thresholds. The combined detection significance is sqrt( sig1**2 + sig2**2 ). --- Sig2 S2-band detection significance number=2 see section 3.5 of the paper for an accurate definition of the acceptance thresholds. The combined detection significance is sqrt( sig1**2 + sig2**2 ). --- Sigc Combined detection significance number=2 see section 3.5 of the paper for an accurate definition of the acceptance thresholds. The combined detection significance is sqrt( sig1**2 + sig2**2 ). --- Detflag Detection flag by number=3 see section 3.4 of the paper. 1 = detection by PSS = Point Source Search program 2 = detection by SESAME = Survey Event Source Analysis by Maximum-likelihood fitting 3 = detection by PSS and SESAME --- u_Detflag 1 indicates uncertainty (:) on Detflag --- VarFlag Variability flag number=4 see section 3.7 of the paper; the variability flag takes the values 0 (no variability claimed); 1 (significant variability); 2 (highly variable). --- EUV Previous reports as EUVE/X-ray source number=5 E=EUVE 1st Catalogue (Bowyer et al. 1994; Catalogue <J/ApJS/93/569>) W=WFC-BSC (Pounds et al. 1993; Catalogue <J/MNRAS/260/77>) X=X-ray, EINSTEIN IPC pointed and/or slew catalogues (Harris et al. 1990; Plummer et al. 1991, CD-ROMs) --- OptName1 Name of possible optical counterpart. --- OptName2 Alternative name of possible optical counterpart. --- SpType Type of counterpart --- Vmag Apparent magnitude of counterpart mag Dist 2RE-optical position difference arcsec r_OptName1 Originating catalogue for counterpart number=6 Extensive use was made of the SIMBAD data-base. The catalogues used are: CVR List of cataclysmic variables compiled by the UK ROSAT CV special interest group in 1990 MCK McCook & Sion (1987) catalogue of spectroscopically identified white dwarf stars (Catalogue <III/129>) SUB Kilkenny, Heber & Drilling (1988, S. Afr. Astron. Obs. Circ. No 12, 1) catalogue of hot subdwarf stars. PUL Lyne pulsar catalogue (e.g. Lyne et al. 1988) (Catalogue <VII/156>) STR Strassmeier et al. (1988) catalogue of chromospherically active binary stars (Catalogue <V/71>). CNS Gliese & Jahreiss (1991) catalogue of nearby stars, 3rd edition, preliminary version (Catalogue <V/70>). GCV General catalogue of variable stars, 4th edition (Kholopov et al. 1988). (Catalogue <II/139>) YAL Bright star catalogue, 5th revised edition, preliminary version (Hoffleit & Warren 1991) (Catalogue <V/50>). LHS Luyten (1976) catalogue of stars with proper motions>0.5arcsec/yr (Catalogue <I/87>) VER Veron-Cetty & Veron (1989) catalogue of quasars and active galactic nuclei (Catalogue <VII/146>). CAT Soifer et al. (1984, ApJ 278, L271) catalogue of galaxies, a merger of various galaxy catalogues. MLN Master hst of non-stellar objects (Dixon & Sonneborn 1980) (Catalogue <VII/2>). SIM Compact version of SIMBAD database. MK Buscombe (1992, "General Catalogue of MK spectral classifications, volumes 7-10, Northwestern University, Evanston Illinois") HIC Hipparcos input catalogue of stars (Turon et al. 1992) (Catalogue <I/196>) GSC HST guide star catalogue (from CD-ROM version 1.1). W ROSAT-WFC Bright Source Catalogue (Pounds et al. 1993). (Catalogue <J/MNRAS/260/77>) E First EUVE source catalogue (Bowyer et al. 1994) (Catalogue <J/ApJS/93/569>). X Einstein IPC point source catalogues, from pointed and slew data (Harris et al. 1990; Plummer et al. 1991; CD-ROMs). --- q_OptName1 Quality of counterpart identification number=7 If this field is blank then any listed possible counterpart is simply based on positional coincidence, and care should be taken in using any such information. IDP+ positive identification, either new, or confirming a catalogued object as the counterpart, resulting from the IDP (Mason et al. 1995, MNRAS 274, 1194) ID** positive identification, based on the properties of the object, either from the existing literature or from follow-up observations other than the IDP, e.g. RS CVn system, or DA white dwarf ID* probable identification, e.g. poorly studied dMe star --- n_OptName1 Notes about the possible counterpart number=8 the following symbols are used: RS (RS CVn-type) (chromospherically/coronally active binaries) BY (BY Dra-type) (chromospherically/coronally active binaries) W (W UMa-type) contact binaries A indicates other active stars --- OClass BROWSE database object class (4 digits). --- catalog.ps The 2RE catalog, PostScript version notes.txt Notes on individual 2RE sources Francois Ochsenbein CDS 1998 Jan 21 UNKNOWN UNKNOWN * 20-Jul-1995: The catalogue was copied in July 1995 via anonymous ftp at: ledas-ftp.star.le.ac.uk and the catalogue file originally named 2re_table.txt was documented according to the CDS Documentation Standards. The notes were converted from the full-paper postscript file (2re_text.ps) * 21-Jan-1998: the flag "note" in byte 14 indicating the existence of a note was added at CDS. J_MNRAS_274_1165.xml Optical identification of EUV sources from the ROSAT Wide Field Camera all-sky survey. J/MNRAS/274/1194 J/MNRAS/274/1194 Optical Identifications of ROSAT EUV Sources Optical identification of EUV sources from the ROSAT Wide Field Camera all-sky survey. K O Mason B J M Hassall G E Bromage D A H Buckley T Naylor D O'Donoghue M G Watson D Bertram G Branduardi-Raymont P A Charles B Cooke K H Elliott M R S Hawkins S T Hodgkin S J Jewell C M Jomaron K Sekiguchi B J Kellett A Lawrence I McHardy J P D Mittaz C D Pike T J Ponman J Schmitt W Voges W Wargau D Wonnacott Mon. Not. R. Astron. Soc. 274 1194 1995 1995MNRAS.274.1194M J/MNRAS/260/77 : ROSAT Wide Field Camera EUV Bright Sources (Pounds+ 1993) J/MNRAS/274/1165 : The 2RE Source Catalogue (Pye+ 1995) Pye J.P. et al., =1995MNRAS.274.1165P Schwartz R.D. et al. =1995PASP..107..667S X-ray sources binaries: general catalogs galaxies: active novae, cataclysmic variables stars: activity white dwarfs Optical identifications for 195 EUV sources located in the ROSAT Wide Field Camera all-Sky survey are presented. We list 69 previous unknown EUV-emitting white dwarfs, 114 active stars, 7 new magnetic cataclysmic variables and 5 active galaxies. Several of the white dwarfs have resolved M-type companions, while five are unresolved white dwarf/M-star pairs. Finding charts are given for the optical counterparts.
ROSAT
WFC optical identification programme ID summary Name Source name --- l_S1 Limit flag on S1 --- S1 WFC survey filter S1 (60-140A) counts 10-3ct/s l_S2 Limit flag on S2 --- S2 WFC survey filter S2 (110-200A) counts 10-3ct/s NH Hydrogen column density --- RAh Right ascension J2000 h RAm Right ascension J2000 min RAs Right ascension J2000 s DE- Declination sign --- DEd Declination J2000 deg DEm Declination J2000 arcmin DEs Declination J2000 arcsec n_DE A 'g' indicates that the data are from the Hubble Space Telescope Guide Star Catalog --- Vmag V magnitude of the optical counterpart mag n_Vmag2 '-' when interval --- Vmag2 Upper limit of Vmag when n_Vmag2='-' mag u_Vmag Uncertainty flag on Vmag --- n_Vmag Note on Vmag number=1 P: CCD or photoelectric photometry (Buckley, private communication; Schwartz et al. 1995) G: The HST Guide Star Catalog (v.1.1) cat: catalogued magnitudes (see Pye et al., 1995) E: POSS E digitized plate material J: SERC J digitized plate material S: uncorrected slit magnitudes taken from calibrated spectra A 'c' appended to the J and E codes indicates that accurate external zero-points were not been obtained by comparing the magnitudes of stars within 3arcmin of the EUV source that appear in the HST Guide Star Catalog (v.1.1) with the uncorrected values measured for those stars from the Schmidt-telescope Sky Survey Plates. If there is more than one counterpart, there are separate entries for each star when these are available. --- B-V B-V color index of the optical counterpart mag SpType Spectral type of the optical counterpart --- l_alpha Limit flag on alpha --- alpha Source apparent EUV to optical flux ratio --- Class Identification class number=2 Star: all active stars WD: white dwarf CV: cataclysmic variable AGN: active galaxy --- EWCa Equivalent width of the Ca H 3933A chromospheric emission line (for stars only) 0.1nm n_EWCa Note on EWCa number=3 u: the line was covered but no measurable emission component was detected. Significant chromospheric emission may still be present, particularly when this refers to Halpha (e.g. the Halpha photospheric absorption line may be 'filled-in' by emission) -: the line was not covered in the spectra --- --- Separator --- EWHa Equivalent width of the Halpha line (for stars only) 0.1nm n_EWHa Note on EWHa number=3 u: the line was covered but no measurable emission component was detected. Significant chromospheric emission may still be present, particularly when this refers to Halpha (e.g. the Halpha photospheric absorption line may be 'filled-in' by emission) -: the line was not covered in the spectra --- FWHb Full width at half maximum of the Hbeta line 10+3km/s --- Separator --- EWHb Equivalent width of the Hbeta line 0.1nm u_EWHb Uncertainty flag on EWHb --- X y: there is an X-ray telescope position available for the source --- Note +: additional information in appena file --- Com Comments --- table1.tex TeX version of table1 Patricia Bauer CDS 1996 Aug 23 K.O. Mason <kom@mssl.ucl.ac.uk> UNKNOWN UNKNOWN In table1, 2RE J033711+255926 was identified to HD 224030 instead of HD 22403. Correction made on 13-Feb-1998. J_MNRAS_274_1194.xml 408-MHz observations of two fields in the region 10h30m, +46deg. I. The surveys J/MNRAS/274/324 J/MNRAS/274/324 408MHz Penticton observations of 51P & 52P 408-MHz observations of two fields in the region 10h30m, +46deg. I. The surveys D A Green J M Riley Mon. Not. R. Astron. Soc. 274 324 1995 1995MNRAS.274..324G J/MNRAS/246/169 : 14P and 15P sources J/A+A/241/551 : 18P and 19P sources J/A+AS/77/31 : 20P and 21P sources J/A+AS/115/345 : 32P and 33P sources Radio sources catalogs radio continuum: general surveys We present results from radio continuum observations of two fields made at 408 and 1420MHz with the DRAO Synthesis Telescope. Two sets of data, one year apart, were obtained of each field, and here we present source lists from the average 408-MHz images, and from the second-epoch 1420-MHz images. Variability studies at 408MHz from these observations will be presented in a forthcoming paper.
1008+46 and 1046+46 fields at 408 and 1240MHz Name Name number=1 51P sources are in 1008+46 field, 52P sources are in 1046+46 field. --- RAh Peak right ascension B1950 h RAm Peak right ascension B1950 min RAs Peak right ascension B1950 s DE- Peak declination sign --- DEd Peak declination B1950 deg DEm Peak declination B1950 arcmin DEs Peak declination B1950 arcsec S408pk Peak flux density at 408MHz mJy S408int Integrated peak density at 408MHz mJy n_S408int See note number=2 In some cases the integration area for one peak may contain other local maxima from the list; where this has occured the integrated flux density will be the same for two or more peaks (indicated by an asterisk) --- S1420pk Peak flux density at 1420MHz mJy S1420int Integrated peak density at 1420MHz mJy n_S1420int See note number=2 In some cases the integration area for one peak may contain other local maxima from the list; where this has occured the integrated flux density will be the same for two or more peaks (indicated by an asterisk) --- Pbm Telescope primary beam response value --- S/N Estimate signal-to-noise ratio of the source --- Patricia Bauer CDS 1996 May 02 The catalogue was provided by Heinz Andernach (R180 in his list) <hja@vilspa.esa.es> Dave Green <dag@mrao.cam.ac.uk> J_MNRAS_274_324.xml The evolution of the quasar luminosity function J/MNRAS/275/1102 J/MNRAS/275/1102 Evolution of quasar luminosity function The evolution of the quasar luminosity function M R S Hawkins P Veron Mon. Not. R. Astron. Soc. 275 1102 1995 1995MNRAS.275.1102H J/MNRAS/260/202 : Quasar luminosity function (Hawkins+, 1993) Magnitudes QSOs Redshifts galaxies: luminosity function, mass function quasars: general In an earlier paper (Hawkins & Veron, 1993MNRAS.260..202H) we presented quasar luminosity functions in three redshift bins, derived from a variability selected sample. Here we provide a major extension to this survey, with a view to improving statistics and completeness, and extending the redshift range. The luminosity functions for redshifts of less than 2.2 show a featureless power law of the form {phi}=10^{beta}(M-M_0_)^, with no sign of a 'break'. The quasar luminosity function is also derived by the redshift range 2.2<z<3.2, which again shows a featureless power law, but with a steeper slope. When the data are combined with a new sample of bright quasars, the quasar luminosity functions in all four redshift ranges are consistent with a single power law of index {beta}=0.63. Plots of quasar space density as a function of redshift in three luminosity bins are also presented and show strong evolution at low redshift but nearly constant space density beyond a redshift of 2.
Quasars in the fibre field sample Quasars in the bright sample Quasars in the high-redshift sample No Quasar number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Bmag B magnitude in 1977 mag U-B U-B color index mag s Variability parameter number=1 The variability parameter s measures the significance of variability and is typically 10 times the amplitude of variation. --- z Redshift --- BMag Absolute B magnitude in 1977 mag James Marcout, Patricia Bauer CDS 1997 Feb 18 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_275_1102.xml The Outer Regions of the Galactic Bulge: I. Observations. J/MNRAS/275/591 J/MNRAS/275/591 Outer regions of Galactic Bulge The Outer Regions of the Galactic Bulge: I. Observations. R A Ibata G Gilmore Mon. Not. R. Astron. Soc. 275 591 1995 1995MNRAS.275..591I Abundances, [Fe/H] Photometry, photographic Radial velocities galaxies: evolution Galaxy: abundances Galaxy: kinematics and dynamics Galaxy: stellar content stars: abundances stars: Population II Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.
The resulting catalogue Name Star Name --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg B-R Photographic photometric colour mag Rmag R-band photographic magnitude mag RVel Mean heliocentric velocity km/s SpClass spectral class number=1 d=dwarf, K=K giant, M=M giant, C=Carbon --- [Fe/H] mean [Fe/H] where repeat data exist Sun Individual observations Name star name --- Obs Year of spectroscopic observation (offset 1900) --- RVel Measured heliocentric velocity km/s SpClass spectral class number=1 d=dwarf, K=K giant, M=M giant, C=Carbon --- [Fe/H] Derived metallicity [Fe/H] Sun Gerry Gilmore ROE Francois Ochsenbein CDS 1995 Mar 15 Gerry Gilmore <gil@ast.cam.ac.uk> J_MNRAS_275_591.xml Spectroscopy for E and S0 galaxies in nine clusters J/MNRAS/276/1341 J/MNRAS/276/1341 Spectroscopy for E and S0 galaxies clusters Spectroscopy for E and S0 galaxies in nine clusters I Jorgensen M Franx P Kjaergaard MNRAS 276 1341 1995 1995MNRAS.276.1341J Clusters, galaxy Galaxies, spectra Central velocity dispersions, Mg2 line indices, and radial velocities for 220 E and S0 galaxies are derived on basis of intermediate resolution spectroscopy. Galaxies in the following clusters have been observed: Abell 194, Abell 539, Abell 3381, Abell 3574, S639, S753, Doradus, HydraI (Abell 1060), and Grm15. The spectra cover 500 or 1000 Angstrom centered on the magnesium triplet at 5177 Angstrom.
In this catalog we give the mean values of the parameters. The central velocity dispersion and the Mg2 line indices have been aperture corrected to a circular aperture with a diameter of 1.19 h^(-1) kpc, equivalent to 3.4arcsec at the distance of the Coma cluster. Values are also given for a circular aperture with radius equal to the effective radius of the galaxy (cf. Jorgensen et al. MNRAS, 273, 1097 (1995)). The Mg2 indices are consistent with the Lick system. The typical uncertainty of the central velocity dispersion is 0.036 in log(sigma), the typical uncertainty of Mg2 is 0.013. Further, literature data (velocity dispersions and Mg2 indices) for the clusters A194, DC2345-28 and Coma (A1656) have been brought on a homogeneous system and aperture corrected to the aperture sizes given above. The literature data are from Davies et al. (ApJS, 64, 581 (1987), Dressler (ApJ, 317, 1 (1987), Dressler & Shectman (AJ, 95, 284 (1988)), Lucey & Carter (MNRAS, 235, 1177 (1988)), Lucey et al. (MNRAS, 253, 584 (1991)), and Guzman et al. (MNRAS, 257, 187 (1992)).
Spectroscopic parameters, new observations Cluster Cluster name --- Galaxy Galaxy name --- RAh Right ascension hours (1950.0) h RAm Right ascension minutes (1950.0) m RAs Right ascension seconds (1950.0) s DE- Sign of declination --- DEd Declination degrees (1950.0) deg DEm Declination minutes (1950.0) arcmin DEs Declination seconds (1950.0) arcsec cz_hel Heliocentric radial velocity km/s lsig_cor log10(sigma), aperture diameter 3.4arcsec at the distance of the Coma cluster (A1656) sigma is the velocity dispersion of the galaxy in km/s. sigma is aperture corrected to the size aperture given in the explanations. --- lsig_re log10(sigma), aperture diameter 2.re, where re is the effective radius in Gunn r --- e_lsig Uncertainty on lsig_cor and lsig_re --- Mg2_lick Mg2 index on Lick system, aperture diameter 3.4arcsec at the distance of the Coma cluster (A1656) Mg2 is the line index of the Mg lines at 5177 Angstrom as defined by Worthey et al. (1994, ApJS, 94, 687). Mg2 is aperture corrected to the size aperture given in the explanations. --- Mg2_re Mg2 index on Lick system, aperture diameter 2.re, where re is the effective in Gunn r --- e_Mg2 Uncertainty on Mg2_lick and Mg2_re --- u_lsig Uncertainty flag on lsig_cor and lsig_re 0 : Signal-to-noise of observation above 20 per Angstrom. 1 : Signal-to-noise of observation below 20 per Angstrom. The velocity dispersion may be affected by systematic errors. --- nobs Number of observations --- Spectroscopic parameters, literature data Cluster Cluster name --- Galaxy Galaxy name --- RAh Right ascension hours (1050.0) h RAm Right ascension minutes (1950.0) min RAs Right ascension seconds (1950.0) s DE- Sign of declination --- DEd Declination degrees (1950.0) deg DEm Declination minutes (1950.0) arcmin DEs Declination seconds (1950.0) arcsec cz_hel Heliocentric radial velocity km/s lsig_cor log10(sigma), aperture diameter 3.4arcsec at the distance of the Coma cluster (A1656) sigma is the velocity dispersion of the galaxy in km/s. sigma is aperture corrected to the size aperture given in the explanations. --- lsig_re log10(sigma), aperture diameter 2.re, where re is the effective radius in Gunn r --- Mg2_lick Mg2 index on Lick system, aperture diameter 3.4arcsec at the distance of the Coma cluster (A1656) Mg2 is the line index of the Mg lines at 5177 Angstrom as defined by Worthey et al. (1994, ApJS, 94, 687). Mg2 is aperture corrected to the size --- Mg2_re Mg2 index on Lick system, aperture diameter 2.re, where re is the effective in Gunn r --- Inger Jorgensen McDonald Observatory, Austin, Texas 1995 Nov 30 J_MNRAS_276_1341.xml Faint UBVRI CCD sequences for wide-field surveys. I. J/MNRAS/276/33 J/MNRAS/276/33 UBVRI CCD sequences for wide-field surveys. I. Faint UBVRI CCD sequences for wide-field surveys. I. B J Boyle T Shanks S M Croom Mon. Not. R. Astron. Soc. 276 33 1995 1995MNRAS.276...33B Photometry, UBVRI Surveys We present the first results of a campaign to secure deep UBVRI CCD photometric calibration in all UK Schmidt equatorial fields with galactic latitudes |b|<~50{deg}. In this paper we provide information on deep BVRI sequences (B<22mag) in 14 UK Schmidt survey fields centred at declination=0{deg}. Deep U sequences have been obtained for 11 of these fields.
UBVRI photometry RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag s/g Star galaxy separation parameter B_5_-B-4_ number=1 Generally, objects with B_5_-B_4_<-0.03 will be galaxies. B_5_-B_4_ is the normalized B frame 4- to 5-pixels aperture correction. --- Umag U magnitude mag e_Umag rms uncertainty on Umag mag Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag Rmag R magnitude mag e_Rmag rms uncertainty on Rmag mag Imag I magnitude mag e_Imag rms uncertainty on Imag mag Patricia Bauer CDS 1999 Apr 21 UNKNOWN UNKNOWN Copied on 22-Apr-1999 at http://icstar5.ph.ic.ac.uk:80/~scroom/phot/photom.html J_MNRAS_276_33.xml IRAS-selected Galactic star-forming regions. - II. Water maser detections in the extended sample J/MNRAS/276/57 J/MNRAS/276/57 IRAS Galactic star-forming regions. II. IRAS-selected Galactic star-forming regions. - II. Water maser detections in the extended sample C Codella G G C Palumbo G Pareschi F Scappini P Caselli M R Attolini Mon. Not. R. Astron. Soc. 276 57 1995 1995MNRAS.276...57C II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) J/A+AS/98/589 : IRAS Sources behind the Solar circle (Wouterloot+ 1993) Infrared sources Masers Radio lines Spectroscopy infrared: ISM: continuum ISM: molecules masers radio lines: ISM stars: formation The results of the analysis of the occurrence of 22.2-GHz H_2_O maser emission in a sample of 1409 IRAS sources north of declination -30deg associated with star-forming regions are presented. Our sample contains all the IRAS sources that satisfy Emerson criteria for selecting molecular cores associated with the earliest evolutionary stages of the star-forming process. In a previous paper (Paper I, 1994MNRAS.266..123P), we have reported the results of the observations of about one third of the sample. In the present paper the observations of the remaining IRAS sources are presented: 18 of them are newly detected maser sources. The results show that 20 per cent of all IRAS sources that satisfy the Wood & Churchwell criteria have H2O water masers. This is in agreement with the assumption that these criteria select objects that are connected with the early phases of the evolution of high-mass star-forming regions. Moreover, about one third of the whole sample selected according to Emerson criteria contains IRAS sources that are not associated with massive star-forming processes, but probably with molecular cores in low-mass star-forming regions.
Subsample A Subsample B Subsample C IRAS IRAS name --- m_IRAS Multilpicity index on IRAS name --- GLON Galactic longitude deg GLAT Galactic latitude deg l_Fpeak Limit flag on Fpeak --- Fpeak Peak flux density Jy n_Fpeak Note on Fpeak number=1 D: Detected as maser by others ND: Not detected as maser by others --- r_Fpeak Fpeak references number=2 References: 1 Present Work 2 Palla et al., 1991A&A...246..249P 3 Felli et al., 1992A&A...255..293F 4 Palla, 1992 (unspecified reference, occurs for IRAS 18134-1652) 5 Comoretto et al., 1990A&AS...84..179C 6 Arcetri Data-base 7 Henning et al., 1992A&AS...93..525H 9 Wouterloot & Walmsley, 1986A&A...168..237W 14 Genzel & Downes, 1977A&A....61..117G 15 Scalise et al., 1989A&A...221..105S 17 Gyulbudaghian et. al., 1990RMxAA..20...51G 19 Wouterloot. et al., 1993A&AS...98..589W, Cat. <J/A+AS/98/589> 20 Palla et al., 1993A&A...280..599P 21 Caswell et al 1983AuJPh..36..443C 22 Churchwell et al., 1990A&ARv...2...79C 23 Knapp & Morris, 1976ApJ...206..713K 24 Jaffe et al., 1981ApJ...250..621J 25 Genzel & Downes, 1979A&A....72..234G 26 Matthews et. al., 1985A&A...149..227M 27 Braz et al., 1989A&AS...77..465B 28 Codella et al., 1994A&A...291..261C 29 Wouterloot et al., 1986A&A...168..237W --- Derived parameters of the new maser sources IRAS IRAS name --- Sample Subsample --- l_F12 Limit flag on F12 --- F12 Flux density at 12{mu}m Jy l_F25 Limit flag on F25 --- F25 Flux density at 25{mu}m Jy l_F60 Limit flag on F60 --- F60 Flux density at 60{mu}m Jy l_F100 Limit flag on F100 --- F100 Flux density at 100{mu}m Jy Date Observing date "DD/MM/YY" Fpeak Flux of the strongest component Jy rms Noise of the spectrum Jy Vpeak Velocity of the strongest component km/s FH2O Integrated flux computed over the whole emission interval Jy.km/s James Marcout, Patricia Bauer CDS 1996 Nov 29 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_276_57.xml A radio-optical survey of the North Ecliptic Cap. J/MNRAS/276/614 J/MNRAS/276/614 Radio-optical 151MHz survey of the N. Ecl. Cap A radio-optical survey of the North Ecliptic Cap. M Lacy J M Riley E M Waldram R G McMahon P J Warner Mon. Not. R. Astron. Soc. 276 614 1995 1995MNRAS.276..614L Radio sources radio continuum: general surveys The Cambridge Low Frequency Synthesis Telescope has been used to survey a region ~7x7deg^2^ about the North Ecliptic Cap at 151MHz with a resolution of 70x77arcsec^2^. The resulting radio source catalogue of 400 sources is complete to a peak flux density limit of 120mJy/beam. Using the Cambridge APM we have searched for identifications on the Palomar Sky Survey plate 550 which covers much of the survey area, and we list the 157 sources with one or more optical objects within 15arcsec of the radio position.
The radio source list Name Radio source name --- m_Name Multiplicity index on name --- RAh Right ascension obtained from beam-fitting (1950) h RAm Right ascension obtained from beam-fitting (1950) min RAs Right ascension obtained from beam-fitting (1950) s DE- Declination sign --- DEd Declination obtained from beam-fitting (1950) deg DEm Declination obtained from beam-fitting (1950) arcmin DEs Declination obtained from beam-fitting (1950) arcsec RAhc Right ascension of source centroid (1950) h RAmc Right ascension of source centroid (1950) min RAsc Right ascension of source centroid (1950) s DE-c Declination sign --- DEdc Declination of source centroid (1950) deg DEmc Declination of source centroid (1950) arcmin DEsc Declination of source centroid (1950) arcsec Flux Flux obtained from beam-fitting Jy FInt Integrated flux Jy S/N Signal-to-noise ratio for each source number=1 Defined as the height of the interpolated maximum on the map divided by the map local noise. --- Extent The extent of the source, in units of the local beam area --- m Number of local maxima within the integration region. --- POSS Result of the APM scan: this is the number of optical objects found on the E550 or O550 POSS plates when the source lies on the area covered by these plates and is -1 otherwise. --- Optical objects within 15 arcsec of the beam-fitted positions Name Radio source name. --- m_Name If there is more than one optical object within 15 arcsec, the optical objects are named 7CXXXX+XXXXa, b , c etc. --- dRA Difference in R.A. between the radio and optical positions arcsec dDE Difference in Dec. between the radio and optical positions arcsec Dist Radial distance between the radio and optical positions arcsec EClass Object classification on the E-plate number=1 -1 for a stellar object +1 for a resolved object +2 for a confused object. A blank indicates a non-detection. --- Emag Magnitude on the E-plate mag OClass Object classification on the O-plate number=1 -1 for a stellar object +1 for a resolved object +2 for a confused object. A blank indicates a non-detection. --- Omag O-magnitude mag l_O-E Limit flag on O-E --- O-E O-E colour mag Notes Notes number=2 Numbers in this column indicate overlap with the sample of Lacy et al., 1993MNRAS.263..707L 1: the optical object is the probable identification according to Lacy et al., 1993MNRAS.263..707L 2: probable mis-identification 3: the special case of 7C1821+6419 (see Lacy et al., 1992MNRAS.258..828L) --- table3.tex LaTeX version of table3 Patricia Bauer CDS 1996 Dec 13 Mark Lacy <m.lacy1@physics.oxford.ac.uk> J_MNRAS_276_614.xml A study of the large-scale distribution of galaxies in the South Galactic Pole region - I. The data. J/MNRAS/276/689 J/MNRAS/276/689 Galaxies in SGP region A study of the large-scale distribution of galaxies in the South Galactic Pole region - I. The data. S Ettori L Guzzo M Tarenghi Mon. Not. R. Astron. Soc. 276 689 1995 1995MNRAS.276..689E Galaxy catalogs Redshifts galaxies: general large-scale structure of universe surveys We present the data from an extensive, moderately deep (b_J_~19.5) spectroscopic survey of ~600 galaxies within four regions of the sky located near the South Galactic Pole. About 75% of the measured galaxies are in an approximately 3x1.5sq.deg region dominated by the rich cluster of galaxies Klemola 44 (Abell 4038). The other three small areas cover about 1sq.deg each. Here, we discuss in detail the observing and data reduction strategies, and the completeness of and errors in the measured redshifts. The data collected are being used for: (i) a study of the large-scale redshift distribution of the galaxies in each field, and (ii) a thorough dynamical investigation of Klemola 44. Results from these analyses will be presented in forthcoming papers.
Redshifts and radial velocities Field Field --- RAh Right ascension B1950 h RAm Right ascension B1950 min RAs Right ascension B1950 s DE- Declination sign --- DEd Declination B1950 deg DEm Declination B1950 arcmin DEs Declination B1950 arcsec bjmag b magnitude mag RV Radial velocity km/s e_RV rms uncertainty on RV km/s z Redshift --- Note Notes --- Patricia Bauer CDS 1996 Apr 29 Luigi Guzzo <guzzo@astmim.mi.astro.it> J_MNRAS_276_689.xml A sample-oriented catalogue of BL Lacertae objects J/MNRAS/277/1477 J/MNRAS/277/1477 A catalogue of BL Lacertae objects A sample-oriented catalogue of BL Lacertae objects P Padovani P Giommi Mon. Not. R. Astron. Soc. 277 1477 1995 1995MNRAS.277.1477P VII/80 : HEAO A-1 (1H) Catalogue VII/152 : the EMSS Catalogue (Gioia et al., 1990) VII/158 : Catalog of QSOs (Hewitt & Burbidge, 1993) VII/175 : Edinburgh-Durham Southern Cluster catalog (Lumsden+ 1992) VII/181 : X-ray of AGNs (Della Ceca+, 1990) VII/188 : Catalog of Quasars and AGN (Veron and Veron, 7th Edition) VIII/5 : The 1Jy Catalog (Kuehr+, 1981) VIII/13 : Catalog of 4.85GHz sources (Becker+ 1991) VIII/27 : Parkes-MIT-NRAO (PMN) surveys (Griffith et al., 1993) J/A+AS/105/211 : Optical identifications of 1Jy (Stickel+ 1994) J/A+AS/109/147 : ROSAT AGN content of 87GB 5 GHz surv. (Brinkmann et al., 1995) BL Lac objects Radio sources X-ray sources BL Lacertae objects: general galaxies: active radio continuum: galaxies X-rays: galaxies We present a catalogue of 233 BL Lacertae objects compiled through an extensive bibliographic search updated to mid-1995. A large fraction of the sources listed in the catalogue belongs to well-defined samples and can be used for statistical purposes. A smaller fraction consists of miscellaneous (but confirmed) BL Lacs and of objects classified as BL Lac candidates. We discuss the selection criteria of the different samples, report the discovery of two previously unnoticed BL Lacs in the Palomar-Green survey, and comment on the possible association of some of the still unidentified high galactic latitude gamma-ray (EGRET, see Thompson et al., =1995ApJS..101..259T) sources with BL Lacs. Some statistical properties of the catalogue are also briefly discussed.
The BL Lac Catalogue (Table 1 of paper) Name Object name(s) --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec u_z Note on redshift: '>' for lower limit, '?' for uncertain, 'd' see number=1 a - Derived from the B magnitude assuming B-V = 0.6, the mean value for BL Lacs b - radio flux at 8.4 GHz c - detected only during phase 2 of the EGRET observations and therefore not included in the phase 1 EGRET catalogue of Fichtel et al. (1994ApJS...94..551F) d - from Murphy, Browne & Perley (1993MNRAS.264..298M); Perlman et al. (1995b, ApJS, in press) give no redshift, so this value might be uncertain e - derived from the mean B magnitude using the observed value of B-V --- z Redshift --- Vmag V magnitude mag n_Vmag Note on V magnitude, see number=1 a - Derived from the B magnitude assuming B-V = 0.6, the mean value for BL Lacs b - radio flux at 8.4 GHz c - detected only during phase 2 of the EGRET observations and therefore not included in the phase 1 EGRET catalogue of Fichtel et al. (1994ApJS...94..551F) d - from Murphy, Browne & Perley (1993MNRAS.264..298M); Perlman et al. (1995b, ApJS, in press) give no redshift, so this value might be uncertain e - derived from the mean B magnitude using the observed value of B-V --- S(5GHz) 5GHz flux mJy n_S(5GHz) Note on radio flux, see number=1 a - Derived from the B magnitude assuming B-V = 0.6, the mean value for BL Lacs b - radio flux at 8.4 GHz c - detected only during phase 2 of the EGRET observations and therefore not included in the phase 1 EGRET catalogue of Fichtel et al. (1994ApJS...94..551F) d - from Murphy, Browne & Perley (1993MNRAS.264..298M); Perlman et al. (1995b, ApJS, in press) give no redshift, so this value might be uncertain e - derived from the mean B magnitude using the observed value of B-V --- Ref References to z, Vmag, S(5GHz) number=2 the references are coded as: B87 =1987A&A...185....9B B90 =1990ApJ...350..578B B92 =1992A&AS...96..339B B94 =1994A&A...286..381B B95 =1995A&AS..109..147B (Catalog <J/A+AS/109/147>) C93 =1993ApJS...85..111C CF94 =1994MNRAS.266..669C D90 =1990ApJS...72..471D (Catalog <VII/181>) E92 =1992ApJS...80..257E F93 =1993AJ....106.1729F F94 =1994ApJS...93..125F FM88 =1988A&AS...76..145F FPT93 =1993ApJ...411L..63F FT90 =1990PASP..102.1120F G86 =1986ApJS...61..305G G91 =1991ApJ...378...77G H91 =1991A&A...248..421H HB93 =1993ApJS...87..451H (Catalog <VII/158>) IPC Einstein IPC database J93 =1993ApJ...404..100J K81 =1981A&AS...45..367K K95 Katgert et al., in prep. KS90 =1990AJ.....99....1K L93 =1993AJ....106..875L M91 =1991ApJ...380...49M M93 =1993MNRAS.264..298M M94 =1994ApL....29..267M N6 =1991ApJS...75....1B (Catalog <VIII/13>) P92 =1992A&A...256..399P P95 =1996ApJ...456..451P PMN Parkes-MIT-NRAO (PMN) Surveys (Catalog <VIII/27>) S89 Schwartz D.A., et al., "BL Lac Objects", Maraschi L., Maccacaro T., Ulrich M.-H., eds, p. 64 S91 =1991ApJ...374..431S S94 =1994A&AS..105..211S (Catalog <J/A+AS/105/211>) SK93 =1993A&AS..101..521S (Catalog <III/175>) SK94 =1994A&AS..103..349S (Catalog <III/175>) ST91 =1991ApJS...76..813S (Catalog <VII/152>) VV93 =1993ESOSR..13....1V (Veron & Veron, Catalog <VII/166>) W95 Wolter et al., in preparation WGA =1994IAUC.6100....1W --- RefX References to X-ray data number=2 the references are coded as: B87 =1987A&A...185....9B B90 =1990ApJ...350..578B B92 =1992A&AS...96..339B B94 =1994A&A...286..381B B95 =1995A&AS..109..147B (Catalog <J/A+AS/109/147>) C93 =1993ApJS...85..111C CF94 =1994MNRAS.266..669C D90 =1990ApJS...72..471D (Catalog <VII/181>) E92 =1992ApJS...80..257E F93 =1993AJ....106.1729F F94 =1994ApJS...93..125F FM88 =1988A&AS...76..145F FPT93 =1993ApJ...411L..63F FT90 =1990PASP..102.1120F G86 =1986ApJS...61..305G G91 =1991ApJ...378...77G H91 =1991A&A...248..421H HB93 =1993ApJS...87..451H (Catalog <VII/158>) IPC Einstein IPC database J93 =1993ApJ...404..100J K81 =1981A&AS...45..367K K95 Katgert et al., in prep. KS90 =1990AJ.....99....1K L93 =1993AJ....106..875L M91 =1991ApJ...380...49M M93 =1993MNRAS.264..298M M94 =1994ApL....29..267M N6 =1991ApJS...75....1B (Catalog <VIII/13>) P92 =1992A&A...256..399P P95 =1996ApJ...456..451P PMN Parkes-MIT-NRAO (PMN) Surveys (Catalog <VIII/27>) S89 Schwartz D.A., et al., "BL Lac Objects", Maraschi L., Maccacaro T., Ulrich M.-H., eds, p. 64 S91 =1991ApJ...374..431S S94 =1994A&AS..105..211S (Catalog <J/A+AS/105/211>) SK93 =1993A&AS..101..521S (Catalog <III/175>) SK94 =1994A&AS..103..349S (Catalog <III/175>) ST91 =1991ApJS...76..813S (Catalog <VII/152>) VV93 =1993ESOSR..13....1V (Veron & Veron, Catalog <VII/166>) W95 Wolter et al., in preparation WGA =1994IAUC.6100....1W --- Sample Sample(s) --- Francois Ochsenbein CDS 1996 Mar 28 Paolo Padovani <padovani@roma2.infn.it> J_MNRAS_277_1477.xml The APM Bright Galaxy Catalogue J/MNRAS/278/1025 J/MNRAS/278/1025 The APM Bright Galaxy Catalogue The APM Bright Galaxy Catalogue J Loveday Mon. Not. R. Astron. Soc.,278,1025 ??? ??? 1996 1996MNRAS.278.1025L Galaxy catalogs Photometry The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.
Galaxies in APM-BGC ID Galaxy name number=1 Each galaxy name is composed of the survey field number and the x, y position of the galaxy on the plate---this should ease location of any particular galaxy on the plate material. The first 3 digits are the SERC field number. The second set of digits are the x-position in millimetres from the centre of the plate (actually the APM scan centre). These are preceded by a `+' sign for galaxies to the right (west) of the plate centre or by a `-' sign for galaxies to the left (east) of centre. The final 3 digits are the y position, again in mm from the plate centre. A preceding `-' indicates galaxies above (north) of the plate centre, `+' indicates galaxies below (south) of the centre. --- RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (arcminutes) arcmin DEs Declination 1950 (arcseconds) arcsec Bj Bj magnitude mag D_MAJ Major diameter arcsec D_MIN Minor diameter arcsec PA Position angle (degrees) number=2 PA is measured clockwise from south-north line. deg MType Morphological type number=3 The morphological type is given by mod(Mtype,10) 1 = Elliptical 2 = Lenticular 3 = Spiral 4 = Irr/Pec 5 = Uncertain 8 = Merged with star 9 = Multile galaxy Galaxies from the ESO catalogue have 10 added. --- Field centres Field SERC field number number= This table lists SERC field centres in 1950 decimal degrees. The column labeled RAextent gives the half-size of the Right Ascension of the field in degrees. The DEextent is 2.5 degrees for every field. This list of fields may be used for example to generate a random catalogue with the same boundaries as the survey data as follows. A point with coordinates (RAp, DEp) is inside a field with coordinates (RAf, DEf) if (abs(RAp - RAf) < RAextent) and (abs(DEp - DEf) < DEextent). An additional test should be made to allow for the extra overlap between fields at RA = 0. If RAf is not zero then abs(RAp) must be greater than RAextent. --- RAdeg RA of field centre 1950 (degrees) number= This table lists SERC field centres in 1950 decimal degrees. The column labeled RAextent gives the half-size of the Right Ascension of the field in degrees. The DEextent is 2.5 degrees for every field. This list of fields may be used for example to generate a random catalogue with the same boundaries as the survey data as follows. A point with coordinates (RAp, DEp) is inside a field with coordinates (RAf, DEf) if (abs(RAp - RAf) < RAextent) and (abs(DEp - DEf) < DEextent). An additional test should be made to allow for the extra overlap between fields at RA = 0. If RAf is not zero then abs(RAp) must be greater than RAextent. deg DEdeg Dec of field centre 1950 (degrees) number= This table lists SERC field centres in 1950 decimal degrees. The column labeled RAextent gives the half-size of the Right Ascension of the field in degrees. The DEextent is 2.5 degrees for every field. This list of fields may be used for example to generate a random catalogue with the same boundaries as the survey data as follows. A point with coordinates (RAp, DEp) is inside a field with coordinates (RAf, DEf) if (abs(RAp - RAf) < RAextent) and (abs(DEp - DEf) < DEextent). An additional test should be made to allow for the extra overlap between fields at RA = 0. If RAf is not zero then abs(RAp) must be greater than RAextent. deg RAextent RA extent of field (degrees) number= This table lists SERC field centres in 1950 decimal degrees. The column labeled RAextent gives the half-size of the Right Ascension of the field in degrees. The DEextent is 2.5 degrees for every field. This list of fields may be used for example to generate a random catalogue with the same boundaries as the survey data as follows. A point with coordinates (RAp, DEp) is inside a field with coordinates (RAf, DEf) if (abs(RAp - RAf) < RAextent) and (abs(DEp - DEf) < DEextent). An additional test should be made to allow for the extra overlap between fields at RA = 0. If RAf is not zero then abs(RAp) must be greater than RAextent. deg Holes drilled around big bright objects Field SERC field number number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif --- HOLX1 RA of 1st corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLY1 Dec of 1st corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLX2 RA of 2nd corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLY2 Dec of 2nd corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLX3 RA of 3rd corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg HOLY3 Dec of 3rd corner of hole (degrees) number= This table lists the coordinates of parallelogram shaped holes drilled out around big bright objects in the survey. The following FORTRAN code will test if a point with coordinates (xr,yr) lies in a hole. c c *** Set drilled = .true. if point (xr,yr) lies in a given hole c c Method: Express displacement vector to (xr,yr) in terms of basis c vectors of parallelogram c c Vr = a1*V1 + a2*V2 c - - - c c Then (xr,yr) is drilled if 0 <= a1,a2 <= 1 c c First, ensure that the RA coords are in [-180,180], since the APM c survey straddles RA = 0. c if (xr.gt.180.0) xr = xr - 360.0 drilled = .false. dx = xr - HOLX1 dy = yr - HOLY1 dx1 = HOLX2 - HOLX1 dy1 = HOLY2 - HOLY1 dx2 = HOLX3 - HOLX1 dy2 = HOLY3 - HOLY1 if (abs(dx2).gt.0) then a1 = (dx*dy2 - dy*dx2)/(dx1*dy2 - dy1*dx2) a2 = (dx - a1*dx1)/dx2 if (0.le.a1.and.a1.le.1.and.0.le.a2.and.a2.le.1) drilled = .true. endif deg Jon Loveday Fermilab 1996 Feb 21 J_MNRAS_278_1025.xml A new large sample of ultraluminous IRAS galaxies. J/MNRAS/279/459 J/MNRAS/279/459 Ultraluminous IRAS galaxies A new large sample of ultraluminous IRAS galaxies. D L Clements W J Sutherland W Saunders G P Efstathiou R G McMahon S Maddox A Lawrence M Rowan-Robinson Mon. Not. R. Astron. Soc. 279 459 1996 1996MNRAS.279..459C II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989) Allen et al. 1991, MNRAS 248, 528 =1991MNRAS.248..528A Huchra's ZCAT, CfA Redshift Catalogue =Catalogue <VII/164> Parker & Watson 1990, A&AS 84, 455 =1990A&AS...84..455P Paturel et al. 1989, A&AS 80, 299 =Catalogue <VII/119> Soifer et al. 1987, Annual Rev. Astron. Astrohpys. 25, 187 Vader & Simon 1987, Nature 327, 304 =1987Natur.327..304V Galaxies, IR galaxies: active galaxies: general infrared: galaxies We present a new, large sample of ultraluminous (L_60_>10^11.4^L_{sun}_ for H_0_=100km/s/Mpc) IRAS galaxies selected for the IRAS Faint Source Survey using a novel optical far-infrared colour selection criterion. Our technique proves to be very successful in selecting luminous galaxies, and we present data on 91 ultraluminous objects, of which 65 are newly discovered. Using our redshift spectra and information from the literature we find that at least 35 per cent of these objects are likely to contain an AGN-type central engine. We also find that purely IR-based techniques for determining the presence of an AGN in these objects are unreliable.
IRAS
Basic data on ultraluminous IRAS galaxies in our new sample Name Object name --- n_Name * indicates the additional object --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec BJmag B_J_ magnitude mag z Redshift --- log(L60) Luminosity at 60um solLum F12 Flux at 12um number=1 A negative value indicates an upper limit Jy F25 Flux at 25um number=1 A negative value indicates an upper limit Jy F60 Flux at 60um Jy F100 Flux at 100um number=1 A negative value indicates an upper limit Jy Ref References number=2 References are: (1) This work (2) Parker & Watson (1990A&AS...84..455P) (3) QDOT (Saunders et al. in preparation) (4) Paturel et al. 1989 <VII/119> (5) Davis et al. private communication (6) Huchra's ZCAT <VII/164> (7) Huchra private communication (8) Soifer et al. 1987, ARA&A 25, 187 (9) Clowes private communication (10) Vader & Simon (1987Natur.327..304V) (11) Allen et al. (1991MNRAS.248..528A) --- Basic information for non-ultraluminous objects discovered in this survey RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s Note * indicates additional object --- DE- Declination sign --- DEd Declinaiton (1950) deg DEm Declinaiton (1950) arcmin DEs Declinaiton (1950) arcsec BJmag B_J_ magnitude mag F60 Flux at 60mum Jy F100 Flux at 100mum number=1 Negative values indicates an upper limit Jy z Redshift --- log(L60) Luminosity at 60mum solLum tables.tex LaTeX version of the tables Patricia Bauer CDS 1996 Aug 22 Dave Clements <dclement@eso.org> J_MNRAS_279_459.xml The 7C Survey of Radio Sources at 151 MHz - a region covering RA 9h to 16h and Dec 20 deg to 35 deg. J/MNRAS/282/779 J/MNRAS/282/779 7C 151-MHz survey of region 9-16h 20-35deg The 7C Survey of Radio Sources at 151 MHz - a region covering RA 9h to 16h and Dec 20 deg to 35 deg. E M Waldram J A Yates J M Riley P J Warner Mon. Not. R. Astron. Soc. 282 779 1996 1996MNRAS.282..779W Radio sources Surveys catalogs surveys The Cambridge Low Frequency Synthesis Telescope has been used at 151 MHz to survey a region of 1393 square degrees, in the range RA 9h to 16h, Dec 20deg to 35deg, with an angular resolution of 108x108cosec(dec) arcsec^2^. The rms noise on the maps is in general ~35-55 mJy/beam but varies considerably and exceeds this in some areas. We have extracted sources with signal-to-noise ratio > 5.5, a total of 5526, and present a catalogue of their positions and flux densities.
7C sourcelist of 5526 sources RAh Beam-fitted position right ascension B1950 h RAm Beam-fitted position right ascension B1950 min RAs Beam-fitted position right ascension B1950 s DE- Beam-fitted position declination (sign) --- DEd Beam-fitted position declination B1950 deg DEm Beam-fitted position declination B1950 arcmin DEs Beam-fitted position declination B1950 arcsec RACh Centroid position right ascension B1950 h RACm Centroid position right ascension B1950 min RACs Centroid position right ascension B1950 s DEC- Centroid position declination (sign) - DECd Centroid position declination B1950 deg DECm Centroid position declination B1950 arcmin DECs Centroid position declination B1950 arcsec S Beam-fitted flux density (Jy/beam) Jy Sint Integrated flux density Jy SNR Signal-to-noise ratio --- Extent Extent of the source in units of local beam area --- Nmax Number of local maxima within the integrated region --- Sally Hales <segh@mrao.cam.ac.uk> MRAO 1996 Jan 12 J_MNRAS_282_779.xml Are the Perseus-Pisces chain and the Pavo-Indus wall connected? J/MNRAS/283/367 J/MNRAS/283/367 Redshift survey in Per-Psc and Pav-Ind Are the Perseus-Pisces chain and the Pavo-Indus wall connected? H Di Nella W J Couch G Paturel Q A Parker Mon. Not. R. Astron. Soc. 283 367 1996 1996MNRAS.283..367D VII/119 : Catalogue of Principal Galaxies (PGC) (Paturel+ 1989) VII/155 : Third Reference Cat. of Bright Galaxies (RC3) Galaxies, optical Redshifts catalogs galaxies: distances and redshifts galaxies: general large-scale structure of universe The list of the measured galaxies is given in Table 3 together with COSMOS coordinates and apparent magnitude. These parameters (plus diameter, axis ratio and position angle) were used to perform cross-identification with the PGC/LEDA objects after reduction to the RC3 system (de Vaucouleurs et al., 1990, see cat. <VII/155>). Both cross correlation results (from `rvsao') and emission line results (from `emsao') are presented. A few galaxies with published redshifts were also observed to derive our external error (see section 3 of the paper).
The measured galaxies RAh Right Ascension 1950 (hours) number=1 Coordinates are from the COSMOS database except for a few cases were positions were taken from the LEDA database. h RAm Right Ascension 1950 (minutes) number=1 Coordinates are from the COSMOS database except for a few cases were positions were taken from the LEDA database. min RAs Right Ascension 1950 (seconds) number=1 Coordinates are from the COSMOS database except for a few cases were positions were taken from the LEDA database. s DE- Declination 1950 (sign) number=1 Coordinates are from the COSMOS database except for a few cases were positions were taken from the LEDA database. --- DEd Declination 1950 (degrees) number=1 Coordinates are from the COSMOS database except for a few cases were positions were taken from the LEDA database. deg DEm Declination 1950 (minutes) number=1 Coordinates are from the COSMOS database except for a few cases were positions were taken from the LEDA database. arcmin DEs Declination 1950 (seconds) number=1 Coordinates are from the COSMOS database except for a few cases were positions were taken from the LEDA database. arcsec Field Internal field number --- Name1 PGC/LEDA number, cat. <I/119> --- Name2 Alternative name number=2 Name in a given hierarchy according to LEDA database: NGC, IC, ESO, MCG (catalogs <VII/62> and <VII/100>) FAIR (Fairall, 1988MNRAS.233..691F), and DRCG (Dressler, 1980ApJS...42..565D, see cat. <VII/174>) --- logD Diameter of major axis in RC3 system 0.1arcmin logR Ratio major/minor axis in RC3 system --- BTmag BT magnitude number=3 BT magnitude from COSMOS database after reduction to the LEDA magnitude system, i.e. BTmag = B(COSMOS) - 0.13 mag PA deg Vcc Heliocentric velocity from cross-correlation method km/s e_Vcc Mean error on Vcc km/s Vem Heliocentric Velocity from emission lines identification method km/s e_Vem Mean error on Vem km/s Notes Notes on the data. --- Francois Ochsenbein CDS 1996 Nov 27 It is a pleasure to thank Helene Di Nella <dinella@mpia-hd.mpg.de> who provided the data to CDS. J_MNRAS_283_367.xml Cross-correlation characteristics of OB stars from IUE spectroscopy. J/MNRAS/284/265 J/MNRAS/284/265 Rotational Velocities of 373 OB stars Cross-correlation characteristics of OB stars from IUE spectroscopy. I D Howarth K W Siebert G A J Hussain R K Prinja Mon. Not. R. Astron. Soc. 284 265 1997 1997MNRAS.284..265H Rotational velocities Spectra, ultraviolet Stars, OB stars: early-type stars: fundamental parameters stars: rotation ultraviolet: stars We present a catalogue of homogeneous measures of the linewidth parameter, v_e_.sin(i), for 373 O-type stars and early supergiants (including the separate components of 25 binary and triple systems), produced by cross-correlating high-resolution, short-wavelength IUE spectra against a `template' spectrum of {tau} Sco. We also tabulate terminal velocities. There are no O supergiants in our sample with v_e_.sin(i)<65km/s, and only one supergiant earlier than B5 has v_e_.sin(i)<50km/s, confirming that an important line broadening mechanism in addition to rotation must be present in these objects. A calibration of the area under the cross-correlation peak against spectral type is used to obtain estimates of continuum intensity ratios of the components in 28 spectroscopically binary or multiple systems. At least seven SB2 systems show evidence for the `Struve-Sahade effect', a systematic variation in relative line strength as a function of orbital phase. The stellar wind of the most rapid rotator in our sample, the O9III:n* star HD 191423 (v_e_.sin(i)<=436km/s), show it to have a `wind-compressed disc' similar to that of HD 93521; this star and other rapid rotators are good candidates for studies of non-radial pulsation.
Velocity Measurements (Table 3 of paper) Name Designation of the star --- SpType Adopted spectral type number=1 generally refers to combined spectrum in binary and multiple systems --- r_SpType Source of spectral type number=2 the source of Spectral Type is coded as follows: CL = Conti & Leep (1974ApJ...193..113C); CLL = Conti, Leep & Lorre (1977ApJ...214..759C); DWC = Dworetsky, Whitelock & Carnochan (1982MNRAS.201..901D); F58 = Feast (1958MNRAS.118..618F); GCM = Garmany, Conti & Massey (1987AJ.....93.1070G); GGR = Georgelin, Georgelin & Roux (1973A&A....25..337G); GHS = Garrison, Hiltner & Schild (1977ApJS...35..111G); HGS = Hiltner, Garrison & Schild (1969ApJ...157..313H); HHC = Houk, Hartoog & Cowley (1976AJ.....81..116H); HKB = Hill, Kilkenny & van Breda (1974MNRAS.168..451H); HMo = Hobbs et al. (1982ApJ...263..690H); H70 = Hill (1970MNRAS.150...23H); MCB = McConnell & Bidelman (1976AJ.....81..225M); MCW = Morgan, Code & Whitford (1955ApJS....2...41M); M88 = Mathys (1988A&AS...76..427M); M89 = Mathys (1989A&AS...81..237M); S70 = Schild (1970ApJ...161..855S); ThA = Thackeray & Andrews (1974A&AS...16..323T); WPN = Walborn, Parker & Nichols (Cat. <III/188>); W72, W73, W76, W81, W82 = Walborn (1972AJ.....77..312W, 1973AJ.....78.1067W, 1976ApJ...205..419W, 1981ApJ...243L..37W, 1982AJ.....87.1300W). --- v.sin(i) V.sin(i) measurement, in km/s km/s u_v.sin(i) Uncertainty flag on v.sin(i) --- v(inf) Terminal wind velocity, in km/s number=1 generally refers to combined spectrum in binary and multiple systems km/s u_v(inf) Uncertaintly flag on v(inf) --- Notes Some alternative designations, and flags '*' for comments in file "notes.dat" number=3 In the notes, "SWP" refers to sequential numbers of images taken with the Short Wavelength Prime camera on the IUE. --- Individual Notes Name Name of star (repeated if several lines) --- Text Text of note --- Ian Howarth UCL Francois Ochsenbein CDS 1997 Jun 30 Ian Howarth <idh@starlink.ucl.ac.uk> Dept. Physics & Astronomy, University College London, Gower St., London WC1E 6BT, UK http://www.star.ucl.ac.uk/~idh J_MNRAS_284_265.xml Radio properties of the Shapley Concentration - I. The Abell cluster A3556 J/MNRAS/285/898 J/MNRAS/285/898 A3556 radio properties Radio properties of the Shapley Concentration - I. The Abell cluster A3556 T Venturi S Bardelli R Morganti R W Hunstead Mon. Not. R. Astron. Soc. 285 898 1997 1997MNRAS.285..898V Clusters, galaxy Radio sources galaxies: clusters: individual (Abell 3556) radio continuum: galaxies We have imaged the portion of the Shapley Concentration core surrounding the cluster A3556 at wavelengths of 36cm with the Molonglo Observatory Synthesis Telescope (MOST), and at 22 and 13cm with the Australia Telescope Compact Array (ATCA). We have defined a radio sample of 112 radio sources at 22cm. Cross-correlation with optical catalogues allowed the identification of 29 radio sources, nine of which belong to A3556. The radio and optical properties of A3556 have been studied in detail. Two extended radio sources are associated with cluster members, i.e. a narrow-angle-tail source located at a projected distance of 0.06R_A_ from the centre, possibly in the late stages of its existence, and a wide-angle-tail source at the periphery of the cluster. We also performed a statistical analysis of the cluster properties. The optical luminosity function shows that the cluster has an excess of bright optical galaxies. In agreement with well-established results, we found that the probability of radio emission increases for brighter galaxies. Furthermore, our radio luminosity function and those obtained for elliptical galaxies located in different environments (poor groups and rich clusters) are very similar, implying that the peculiar dynamical state of A35S6 has no influence on the radio emission properties of the cluster galaxies.
Source list and flux density values Name Source name --- m_Name Multiplicity index on Name --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec S22cm 22cm flux density (1.4GHz) mJy S13cm 13cm flux density (2.3GHz) mJy S36cm 36cm flux density (0.83GHz) mJy Morph Radio morphology number=1 The morphologies refer to the 22-cm mosaic map. D* indicates that the source is a double, and the position given is that of the radio barycentre. --- n_Morph Note on Morph number=2 a: this source was detected in the large 1.5D map, but it is out of the final mosaic map. --- Radio and optical data for the optical identifications. RName Radio name --- RArh Radio right ascension (2000) h RArm Radio right ascension (2000) min RArs Radio right ascension (2000) s DEr- Radio declination sign --- DErd Radio declination (2000) deg DErm Radio declination (2000) arcmin DErs Radio declination (2000) arcsec S22cm 22cm flux density mJy radType Radio type number=1 *: stellar appearance; classified as star in the COSMOS catalogue. +: flagged in the COSMOS catalogue as too 'faint'. --- DRO Difference between radio and optical centres arcsec n_DRO When *, see note number=3 Individual notes: J1321-3042: This radio source was detected in the 1.5D map, owing to the large field. It is out of the final mosaic map. J1321-3130: The source is the edge of our mosaic map, therefore uncertainties in the image could be larger than in the rest of the field. The appearance is that of a classical double source with a optical object between the two components. The radio position is that of the radio barycentre. J1322-3114: Classical double source (FRII) with an object between the two components. J1322-3128: Classical double source (FRI/II) with a faint object between the two components. J1323-3150: Very extended optical galaxy, see Section 5 in the text. J1324-3138: Extended radio source discussed in section 6.1 --- OName Optical name --- RAoh Optical right ascension (2000) h RAom Optical right ascension (2000) min RAos Optical right ascension (2000) s DEo- Optical declination sign --- DEod Optical declination (2000) deg DEom Optical declination (2000) arcmin DEos Optical declination (2000) arcsec Bjmag Apparent b_J_ magnitude mag n_Bjmag Note on Bjmag number=2 D stands for double radio morphology (see also Table 3), E for elliptical galaxy. --- optType Optical type --- Vel Recession velocity km/s n_Vel Q: Velocities taken from Quintana et al. (1995, Cat. <J/AJ/110/463>). --- Note When *, see note number=3 Individual notes: J1321-3042: This radio source was detected in the 1.5D map, owing to the large field. It is out of the final mosaic map. J1321-3130: The source is the edge of our mosaic map, therefore uncertainties in the image could be larger than in the rest of the field. The appearance is that of a classical double source with a optical object between the two components. The radio position is that of the radio barycentre. J1322-3114: Classical double source (FRII) with an object between the two components. J1322-3128: Classical double source (FRI/II) with a faint object between the two components. J1323-3150: Very extended optical galaxy, see Section 5 in the text. J1324-3138: Extended radio source discussed in section 6.1 --- James Marcout, Patricia Bauer CDS 1997 Oct 21 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_285_898.xml Quantitative Spectral Classification of Galactic Disk K-M Stars from Spectrophotometric Measurements J/MNRAS/286/500 J/MNRAS/286/500 Classification of Late Type Stars Quantitative Spectral Classification of Galactic Disk K-M Stars from Spectrophotometric Measurements V Malyuto M O Oestreicher Th Schmidt-Kaler Mon. Not. R. Astron. Soc. 286 500 1997 1997MNRAS.286..500M Spectrophotometry Stars, supergiant stars: fundamental parameters stars: late-type Energy distributions for 33 galactic (super)giants situated mostly in the southern Milky Way in the range from 4800 to 7700 Angstroems with an effective resolution of 10 Angstroems are presented here. The observations and reductions are described in the paper. The errors of the absolute and relative flux calibration are 0.028 and 0.021 mag, respectively. The S/N ratio is at least 80 for each star. Cross references, MK classifications and spectral indices one may find in the paper. Further informations are available at M.O.Oestreicher (mio@astro.ruhr-uni-bochum.de). The data are given in three files: 1) stars.dat A list of the programme stars listing the HD/HDE numbers, MK types and positions related to J2000 2) absolute.dat A list of absolute fluxes for each star observed under photometric conditions (18 stars). The fluxes are given in magnitudes according to the system of Hayes & Latham (1975). A monochromatic magnitude of 0.00 corresponds to a flux of 3.5x10^-20^ erg.cm-2.s-1.Hz-1, (3.5x10^-23^ W/m2/Hz), i.e. the fluxes are related to FREQUENCY INTERVALS. 3) relative.dat A list of relative fluxes for each star observed in nights of low quality (15 stars). The fluxes are normalized to 1 at 5555 Angstr. and are related to WAVELENGTH INTERVALS.
List of programme stars HD HD/HDE number --- SpType MK spectral type --- MKlum MK luminosity class + peculiarities --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec List of absolute fluxes for each star observed under photometric conditions lambda Wavelength 0.1nm mag14 Absolute flux for HD 89845 mag mag15 Absolute flux for HD 90382 mag mag17 Absolute flux for HD 91093 mag mag18 Absolute flux for HD 93281 mag mag19 Absolute flux for HD 93420 mag mag20 Absolute flux for HD 94096 mag mag21 Absolute flux for HD 94599 mag mag22 Absolute flux for HD 94613 mag mag23 Absolute flux for HD 95687 mag mag24 Absolute flux for HD 95950 mag mag25 Absolute flux for HD 97671 mag mag26 Absolute flux for HD 98817 mag mag27 Absolute flux for HD 99619 mag mag28 Absolute flux for HD 100930 mag mag29 Absolute flux for HD 101007 mag mag30 Absolute flux for HD 101712 mag mag32 Absolute flux for HD 300933 mag mag33 Absolute flux for HD 303250 mag List of relative fluxes for all other stars lambda Wavelength 0.1nm Flux01 Relative flux (to 5555A) for HD 33299 --- Flux02 Relative flux (to 5555A) for HD 35601 --- Flux03 Relative flux (to 5555A) for HD 37387 --- Flux04 Relative flux (to 5555A) for HD 42474 --- Flux05 Relative flux (to 5555A) for HD 42475 --- Flux06 Relative flux (to 5555A) for HD 42543 --- Flux07 Relative flux (to 5555A) for HD 44213 --- Flux08 Relative flux (to 5555A) for HD 44391 --- Flux09 Relative flux (to 5555A) for HD 48640 --- Flux10 Relative flux (to 5555A) for HD 49068 --- Flux11 Relative flux (to 5555A) for HD 58061 --- Flux12 Relative flux (to 5555A) for HD 65412 --- Flux13 Relative flux (to 5555A) for HD 81137 --- Flux16 Relative flux (to 5555A) for HD 90586 --- Flux31 Relative flux (to 5555A) for HD 103052 --- Michael Oestreicher Bochum Francois Ochsenbein CDS 1997 Apr 25 J_MNRAS_286_500.xml Evidence for a new class of extreme ultraviolet sources J/MNRAS/287/293 J/MNRAS/287/293 BR photometry of EUVE sources Evidence for a new class of extreme ultraviolet sources D Maoz E O Ofek A Shemi Mon. Not. R. Astron. Soc. 287 293 1997 1997MNRAS.287..293M J/ApJS/93/569 : First EUVE source catalogue (Bowyer+, 1994) II/203 : Second Extreme Ultra-Violet Explorer Catalog (2EUVE, 1996) J/MNRAS/274/1165 : The 2RE Source Catalogue (Pye+ 1995) Photometry Ultraviolet X-ray sources novae, cataclysmic variables stars: activity stars: neutron white dwarfs X-rays: stars Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.
Unidentified EUV sources EUVE EUV source name (EUVE or RE) --- Band EUV band --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec GLON Galactic longitude deg GLAT Galactic latitude deg Date Observation date "DD/MM/YY" Bexp Time of B exposition s Rexp Time of R exposition s BR photometry for unidentified EUV sources EUVE EUV source name --- Star Star number in the EUVE field --- Sep Separation arcsec oRA Offset in right ascension number=1 Positions (J2000) are relative to: RA=07h15m50s, DE=+14{deg}10'18" for EUVE 0715+141 RA=08h07m59s, DE=+21{deg}04'12" for EUVE 0807+210 RA=08h47m13s, DE=+59{deg}47'00" for RE 0847+594 RA=09h22m29s, DE=+71{deg}10'06" for EUVE 9022+711 RA=16h36m34s, DE=-28{deg}32'00" for EUVE 1636-285 RA=20h53m35s, DE=-17{deg}33'54" for EUVE 2053-175 RA=21h14m41s, DE=+50{deg}18'12" for EUVE 2114+503 arcsec oDE Offset in declination number=1 Positions (J2000) are relative to: RA=07h15m50s, DE=+14{deg}10'18" for EUVE 0715+141 RA=08h07m59s, DE=+21{deg}04'12" for EUVE 0807+210 RA=08h47m13s, DE=+59{deg}47'00" for RE 0847+594 RA=09h22m29s, DE=+71{deg}10'06" for EUVE 9022+711 RA=16h36m34s, DE=-28{deg}32'00" for EUVE 1636-285 RA=20h53m35s, DE=-17{deg}33'54" for EUVE 2053-175 RA=21h14m41s, DE=+50{deg}18'12" for EUVE 2114+503 arcsec Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag Rmag R magnitude mag e_Rmag rms uncertainty on Rmag mag B-R B-R colour mag e_B-R rms uncertainty on B-R mag X-ray visibility of EUV-detected CVs Name Star name --- Type Stellar type --- EUVE100 EUVE survey at 100{AA} counts ct/ks n_EUVE100 *: EUVE observations with the Deep Survey Telescope --- e_EUVE100 rms uncertainty on EUVE100 ct/ks EUVE200 EUVE survey at 200{AA} counts ct/ks e_EUVE200 rms uncertainty on EUVE200 ct/ks EUVE400 EUVE survey at 400{AA} counts ct/ks e_EUVE400 rms uncertainty on EUVE400 ct/ks EUVE600 EUVE survey at 600{AA} counts ct/ks e_EUVE600 rms uncertainty on EUVE600 ct/ks WFC100 ROSAT WFC survey at 100{AA} counts ct/ks e_WFC100 rms uncertainty on WFC100 ct/ks WFC150 ROSAT WFC survey at 150{AA} counts ct/ks e_WFC150 rms uncertainty on WFC150 ct/ks XRT ROSAT XRT survey at 0.1-2.4keV counts ct/ks e_XRT rms uncertainty on XRT ct/ks tables.tex LaTeX version of the tables James Marcout, Patricia Bauer CDS 1997 Oct 24 Dan Maoz <dani@wise.tau.ac.il> J_MNRAS_287_293.xml Unveiling a connection between large-scale structures behind the southern Milky Way J/MNRAS/287/472 J/MNRAS/287/472 Southern Milky Way galaxies velocities Unveiling a connection between large-scale structures behind the southern Milky Way H Di Nella W J Couch Q A Parker G Paturel Mon. Not. R. Astron. Soc. 287 472 1997 1997MNRAS.287..472D VII/119 : Catalogue of Principal Galaxies (PGC) (Paturel+ 1989) J/A+AS/117/519 : Structures around the SGP (Escalera+, 1996) Galaxy catalogs Morphology Space velocities catalogs galaxies: distances and redshifts large-scale structure of universe A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (<http://www-obs.univ-lyon1.fr/base/>) and COSMOS (Cat. <J/A+AS/117/519>) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5<B_J_<17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.
The 211 measured galaxies. RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec PGC PGC/LEDA number (Paturel et al., 1989, Cat. <VII/119>) --- Name Alternative names --- logD log of the major axis of the galaxy from LEDA database [arcmin] logR log of the axis ratio from LEDA database --- BT B_T_ magnitude from LEDA database mag Vleda Heliocentric velocity km/s a Major axis from COMOS database arcsec b Minor axis from COMOS database arcsec PA Position angle, from COMOS database, measured from the North to the East deg BJmag B_J_ magnitude from COMOS database mag HVel Heliocentric velocity from this survey km/s n_HVel Notes number=1 : indicates poor determination of the redshift c indicates a conflictual measurement against a previous one i indicates a conflictual identification. --- James Marcout, Patricia Bauer CDS 1997 Oct 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_287_472.xml The Edinburgh-Cape Blue Object Survey - II. Zone 1 - the North Galactic Cap J/MNRAS/287/867 J/MNRAS/287/867 Edinburgh-Cape Blue Object Survey. Zone 1. The Edinburgh-Cape Blue Object Survey - II. Zone 1 - the North Galactic Cap D Kilkenny D O'Donoghue C Koen R S Stobie A Chen Mon. Not. R. Astron. Soc. 287 867 1997 1997MNRAS.287..867K Blue objects Photometry, UBV Surveys quasars: general stars: early-type stars: horizontal-branch subdwarfs surveys white dwarfs Results for Zone 1 of the Edinburgh-Cape (EC) Blue Object Survey are presented. This zone covers that part of the North Galactic Cap more than ~30{deg} from the Galactic plane and south of about -12.3{deg} declination (although a few fields north of this declination are included). The zone effectively complements the Palomar-Green Survey in the North Galactic Cap, although the EC Survey should be more complete to a fainter limit (B=16.5mag) and to somewhat redder stars (U-B bluer than about -0.4). Zone 1 covers approximately 1560{deg}^2^ and contains 675 blue objects far which we list equatorial coordinates accurate to ~1arcsec, UBV photoelectric photometry, and spectral types determined from moderate-dispersion (100{AA}/mm) spectrograms.
Catalogue of Edinburgh-Cape Survey blue objects from Zone I - The North Galactic Cap. Catalogue of Edinburgh-Cape Survey F/G stars from Zone 1. EC EC number --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Date Observation date "DD/MM/YY" Vmag V magnitude mag u_Vmag Uncertainty flag on Vmag --- B-V B-V colour index mag u_B-V Uncertainty flag on B-V --- U-B U-B colour index mag u_U-B Uncertainty flag on U-B --- SpType Spectral type --- Com Comments, an '*' indicates a note number=1 K91: Kilkenny et al., 1991MNRAS.248..664K --- Additional notes to table1.dat Additional notes to table2.dat EC EC number, repeated for continuation lines --- Text Text of Comment --- James Marcout, Patricia Bauer CDS 1998 May 11 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_MNRAS_287_867.xml An H I aperture synthesis mosaic of the Small Magellanic Cloud J/MNRAS/289/225 J/MNRAS/289/225 SMC HI shells velocities An H I aperture synthesis mosaic of the Small Magellanic Cloud L Staveley-Smith R J Sault D Hatzidimitriou M J Kesteven D McConnell Mon. Not. R. Astron. Soc. 289 225 1997 1997MNRAS.289..225S H I data Magellanic Clouds Radial velocities galaxies: kinematics and dynamics ISM: atoms ISM: kinematics and dynamics Magellanic Clouds radio lines: ISM surveys We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales <=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size >=0.6{deg}, and should not be used for deriving total H I column densities
List of positions, radii, expansion velocities, ages and required wind luminosities for the H I shells identified in the SMC SSH97 SMC HI shell number --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Rad1 Shell angular radius arcmin u_Rad1 Uncertainty flag on Rad1 --- Rad2 Shell linear radius pc HV Central heliocentric velocity km/s u_HV Uncertainty flag on HV --- Vexp Expansion velocity number=1 Expansion velocity (km/s) (half the width between the red-shifted and blue-shifted peaks) km/s u_Vexp Uncertainty flag on Vexp --- Age Dynamical age Myr log(Ls/n0) Required mechanical wind luminosity number=2 Ls=1.5*10^5^(rs/100pc)^5^(Ts/10^6^yr)^-3^(no/1cm^-3^)L_{sun}_ where Ls is the wind velocity, Ts the dynamical age (in yr), rs the radius (in pc) and no the ambient density [solLum.cm+3] James Marcout, Patricia Bauer CDS 1997 Oct 24 Lister Staveley-Smith <lstavele@atnf.CSIRO.AU> J_MNRAS_289_225.xml The APM galaxy survey - V. Catalogues of galaxy clusters. J/MNRAS/289/263 J/MNRAS/289/263 Galaxy clusters from the APM galaxy survey The APM galaxy survey - V. Catalogues of galaxy clusters. G B Dalton S J Maddox W J Sutherland G Efstahiou Mon. Not. R. Astron. Soc. 289 263 1997 1997MNRAS.289..263D J/MNRAS/278/1025 : The APM Bright Galaxy Catalogue (Loveday 1996) J/MNRAS/246/433 : APM galaxy survey. II. (Maddox+ 1990) J/MNRAS/269/151 : APM galaxy survey. IV. (Dalton+, 1994) J/MNRAS/274/1071 : Edinburgh-Milano cluster redshift survey (Collins+ 1995) VII/203 : Las Campanas Redshift Survey (Shectman+ 1996) Maddox et al., Paper I. 1990MNRAS.243..692M Maddox et al., Paper II. 1990MNRAS.246..433M, Cat. <J/MNRAS/246/433> Maddox et al., Paper III. 1996MNRAS.283.1227M Dalton et al., Paper IV. 1994MNRAS.269..151D, Cat. <J/MNRAS/269/151> Clusters, galaxy catalogs galaxies: clusters: general large-scale structure of universe surveys We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.
The APM cluster catalogue Cluster Cluster number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Xmag X magnitude number=1 We define Xmag to be the magnitude for which C_i_=X, i.e. in the case of X=10 with no weighting then Xmag is exactly equivalent to Abell's m_10_. (C_i_ is the weighted sum of galaxies brighter than m_i_ minus the expected background count brighter than m_i_.) mag rC Projected radius arcmin z Estimated redshift determined from Xmag --- R Cluster richness --- n_R Notes number=2 a: This cluster is close to a bright star which has been excised from the galaxy catalogue. A part of the cluster area is therefore missing from the survey data and so the richness may have been underestimated. b: The field of this cluster includes a 2-arcmin foreground galaxy 0.7r_C_ from the centre which has been broken up into several small galaxian images by the APM software. These additional objects may have caused the richness to be slightly overestimated. c: This field is dominated by a 2-arcmin foreground galaxy which has been broken up into several small galaxian images by the APM software. The field does not appear to contain a true cluster. The cluster was below the richness threshold used by Dalton et al. (1994MNRAS.271L..47D) and was not visually inspected at the time of those observations. --- zabs Absorption redshift --- n_zabs Notes number=3 1: Redshift from Paper IV, Dalton et al., 1994, Cat. <J/MNRAS/269/151> 2: Redshift measured by Dalton et al. (1994MNRAS.271L..47D). Note that this survey was limited to Xmag <=19.2 3: Redshift measured as part of the deep extension to the APM cluster redshift survey (Croft et al., 1997, MNRAS, in press) 4: Cluster found in the Edinburgh-Milano Cluster Redshift Surcey (Collins et al., 1995, Cat. <J/MNRAS/274/1071>). If only one references is present then the redshift is adopted from this source, otherwise this entry indicates that the cluster is also found in that survey. 5: Cluster redshift has been drawn from Las Campanas Redshifdt Survey (LCRS: Schectman et al., 1996ApJ...470..172S. Cat. <VII/203>) +: For the cluster APM 100, we have adopted the value given by Collins et al. (1995, Cat. <J/MNRAS/274/1071>) as they point out this is in better agreement with the maximum likelihood redshift estimate quoted in Paper IV (Cat. <J/MNRAS/269/151>) than our single galaxy redshift. --- Patricia Bauer CDS 1997 Oct 10 Gavin Dalton <g.dalton1@physics.ox.ac.uk> J_MNRAS_289_263.xml Red supergiants in the LMC. I. BVRIJHK photometry, magnitudes and intrinsic colours. J/MNRAS/289/729 J/MNRAS/289/729 BVRIJHK photometry of red LMC supergiants Red supergiants in the LMC. I. BVRIJHK photometry, magnitudes and intrinsic colours. M O Oestreicher T Schmidt-Kaler W Wargau Mon. Not. R. Astron. Soc. 289 729 1997 1997MNRAS.289..729O Photometry, UBVRIJKLMNH Stars, late-type Stars, supergiant Magellanic Clouds stars: fundamental parameters stars: late-type supergiants (BV)_J_(RI)_C_ observations for 185 and additional JHK observations for 53 red supergiant candidates in the Large Magellanic Cloud (LMC) are presented. The data have been reduced discussing carefully the dependence of effective wavelengths on the spectral energy distribution of the star, which is very strong especially for the Cousins R band. Non-linear colour dependences of transformation coefficients vor the V magnitude and the R-I colour have been taken into account. The mean error of the BVRI data is 0.03 to 0.04 mag, while that of the JHK observations is 0.02mag. The MK types are not given to the stars, as the classifications given in the literature are mostly very uncertain. The spectra we have obtained for 88 of the stars will be discussed in a forthcoming paper where we will give directly physical properties like Mbol and Teff instead of MK types. Most of the stars are supergiants of type late K to early M.
BVRI photometry (table 4 of paper) Star Identification SP = Sanduleak & Philip (1977) FD = Fehrenbach & Duflot (1970A&ASS...1....1F) RM = Rebeirot et al. (1983A&AS...51..277) --- WOH Identification number according to Westerlund et al. (1981A&AS...43..267W) --- RM Identification number according to Rebeirot et al. (1983A&AS...51..277) --- HV Harvard variable identification number --- RAh Right Ascension 1975 (hours) h RAm Right Ascension 1975 (minutes) min RAs Right Ascension 1975 (seconds) s DE- Declination 1975 (sign) --- DEd Declination 1975 (degrees) deg DEm Declination 1975 (minutes) arcmin DEs Declination 1975 (seconds) arcsec Vmag V magnitude mag e_Vmag Error of Vmag mag B-V B-V colour mag e_B-V Error of B-V mag V-R V-R colour mag e_V-R Error of V-R mag R-I R-I colour mag e_R-I Error of R-I mag Nobs Number of measurements --- Jflag when JHK photometry exists in jhk.dat --- Rem Remark flags Stars with one asterisk have been identified spectroscopically as foreground stars. Stars with two asterisk have uncertain photometries due to extrapolation of the transformation. --- JHK photometry (table 9 of paper) Star Identification, as in file bvri.dat --- Jmag J magnitude mag e_Jmag Error of Jmag mag J-H J-H colour mag e_J-H Error of J-H colour mag H-K H-K colour mag e_H-K Error of H-K colour mag Rem Remark flags Stars with one asterisk have been identified spectroscopically as foreground stars. Stars with two asterisk have probably uncertain photometries due to bad weather and technical problems. --- Francois Ochsenbein CDS 1998 Oct 26 Michael Oestreicher <mio@astro.ruhr-uni-bochum.de> UNKNOWN UNKNOWN * 30-Sep-1997: data kindly supplied by Michael Oestreicher (mio@astro.ruhr-uni-bochum.de) * 26-Oct-1998: Corrections in the following records of bvri.dat: #013: HV number is 5498 instead of 5499 #109: WOH number is S338 instead of S388 #151: position, WOH and RM numbers corrected. #185: WOH number corrected. J_MNRAS_289_729.xml Studies of ultracompact H II regions. I. Methanol maser survey of IRAS-selected sources. J/MNRAS/291/261 J/MNRAS/291/261 Methanol maser of IRAS-selected sources Studies of ultracompact H II regions. I. Methanol maser survey of IRAS-selected sources. A J Walsh A R Hyland G Robinson M G Burton Mon. Not. R. Astron. Soc. 291 261 1997 1997MNRAS.291..261W J/ApJS/91/659 : Ultracompact HII regions radio images (Kurtz+ 1994) J/A+AS/110/81 : Methanol masers towards IRAS sources (van der Walt+ 1995) H II regions Masers Radial velocities HII regions ISM: molecules radio lines: ISM stars: formation surveys A survey of ultracompact (UC) HII regions has been carried out by searching for 6.669-GHz methanol maser emission from a sample of 535 IRAS-selected candidates. A total of 201 candidates exhibit methanol emission. These sources have been used, in conjunction with previously identified UC HII regions, to provide a base for further studies of such regions. Estimates of distances have indicated that the identified UC HII regions tend to have some Galactic structure but it is not clear whether they lie in or between the spiral arms of the Galaxy. The regions are tightly constrained to the plane of the Galaxy. Comparison of identified regions and IRAS sources selected by Wood & Churchwell indicates that there there is some degree of contamination, which could be due to an older phase in the life on an UC HII region where methanol maser emission is not apparent. Luminosities and spectral types have been derived for many of the regions. The maximum number of maser spots observed seems to increase with increasing peak maser luminosity, which indicates that the maser emission is more dependent on the abundance of methanol than the availability of far-infrared radiation.
IRAS sources in our data set with no positive methanol identification, and no other defining UC H II characteristics IRAS IRAS PSC name (Cat. <II/125>) --- List of the 215 candidates identified as UC H II regions IRAS IRAS PSC name (Cat. <II/125>) --- GLON Galactic longitude of pointing centre number=1 Galactic coordinates are shown in degrees and are derived from the (B1950) positions or from Caswell et al. (1995MNRAS.272...96C), where the data of Caswell et al. has been used in columns Peak to Npeak (see Note (2)) deg GLAT Galactic latitude of pointing centre number=1 Galactic coordinates are shown in degrees and are derived from the (B1950) positions or from Caswell et al. (1995MNRAS.272...96C), where the data of Caswell et al. has been used in columns Peak to Npeak (see Note (2)) deg Peak Peak flux density of methanol maser emission Jy n_Peak Note on observation of Peak number=2 The methanol maser data provided in columns Peak to Npeak come from three different observation times. a: Data obtained during the period 24-27 September 1993 b: Data obtained during the period 8-12 April 1994 and the remaining is that published by Caswell et al. (1995MNRAS.272...96C) g: Object also been observed by Schutte et al. (1993MNRAS.261..783S) A comparison indicates that our observation position was not accurately centred on the maser emission, since our maser peak flux densities are substantially lower than that of Schutte et al. (1993MNRAS.261..783S) --- RV Radial velocity of Peak maser component km/s Vinf Velocity range over which maser emission is seen (lower value) km/s Vsup Velocity range over which maser emission is seen (upper value) km/s n_Vsup Note on Velocity range number=3 d: Source that probably have more than one methanol emission peak, due to the broad velocity range, but only one maser spot can be unambiguously identified in the spectrum. --- Npeak Number of maser peaks observed in each spectrum --- Dist Adopted kinematic distance number=4 The distances given are determined kinematically, using the methanol maser velocity, except for those sources where r_Dist = e or z. The distances obtained from previous papers tend to agree approximately with our kinematic distance where the kinematic distance could be measured. kpc Dist2 Second kinematic distance when ambiguity kpc r_Dist Source of Dist number=5 e: Distances obtained from Table 4 of Wood & Churchwell (1989ApJS...69..831W) z: Distances obtained from Table 2 of Kurtz et al. (1994, Cat. <J/ApJS/91/659>) i: Sources that have no distance estimate due to the large uncertainties --- Ltot Calculated total luminosity for IRAS fluxes form Dist value 10+4solLum Ltot2 Calculated total Luminosity for IRAS fluxes from Dist2 value 10+4solLum SpType Spectral type of single star responsible for emission in Ltot --- SpType2 Spectral type of single star responsible for emission in Ltot2 --- Ass1 Other association number=6 M: previous methanol maser detection O: previous OH maser detection W: previous water maser detection U: previous identification by a compact radio source N: sources discovered in this paper or reported in Walsh et al. (1995PASA...12..186W) x: non-detection in methanol emission by us --- r_Ass1 Source of Ass1 number=7 e: Henning et al. (1992A&AS...93..525H) f: Kurtz et al. (1994, Cat. <J/ApJS/91/659>) g: Churchwell (1990A&ARv...2...79C) h: Wood & Churchwell (1989ApJS...69..831W) j: Caswell et al. (1995MNRAS.272...96C) k: Braz et al. (1990A&A...236..479B) l: MacLeod & Gaylard (1992MNRAS.256..519M) m: Schutte et al. (1993MNRAS.261..783S) n: van der Walt et al. (1995, Cat. <J/A+AS/110/81>) p: Caswell et al. (1995MNRAS.277..210C) q: Norris et al. (1987ApJ...321L.159N) r: Kemball et al. (1988ApJ...331L..37K) s: Ellingsen et al. (1996MNRAS.280..378E) t: Forster & Caswell (1989A&A...213..339F) u: Cesaroni et al. (1991A&A...252..278C) v: Palla et al. (1991A&A...246..249P) --- Ass2 Other association number=6 M: previous methanol maser detection O: previous OH maser detection W: previous water maser detection U: previous identification by a compact radio source N: sources discovered in this paper or reported in Walsh et al. (1995PASA...12..186W) x: non-detection in methanol emission by us --- r_Ass2 Source of Ass2 number=7 e: Henning et al. (1992A&AS...93..525H) f: Kurtz et al. (1994, Cat. <J/ApJS/91/659>) g: Churchwell (1990A&ARv...2...79C) h: Wood & Churchwell (1989ApJS...69..831W) j: Caswell et al. (1995MNRAS.272...96C) k: Braz et al. (1990A&A...236..479B) l: MacLeod & Gaylard (1992MNRAS.256..519M) m: Schutte et al. (1993MNRAS.261..783S) n: van der Walt et al. (1995, Cat. <J/A+AS/110/81>) p: Caswell et al. (1995MNRAS.277..210C) q: Norris et al. (1987ApJ...321L.159N) r: Kemball et al. (1988ApJ...331L..37K) s: Ellingsen et al. (1996MNRAS.280..378E) t: Forster & Caswell (1989A&A...213..339F) u: Cesaroni et al. (1991A&A...252..278C) v: Palla et al. (1991A&A...246..249P) --- Ass3 Other association number=6 M: previous methanol maser detection O: previous OH maser detection W: previous water maser detection U: previous identification by a compact radio source N: sources discovered in this paper or reported in Walsh et al. (1995PASA...12..186W) x: non-detection in methanol emission by us --- r_Ass3 Source of Ass3 number=7 e: Henning et al. (1992A&AS...93..525H) f: Kurtz et al. (1994, Cat. <J/ApJS/91/659>) g: Churchwell (1990A&ARv...2...79C) h: Wood & Churchwell (1989ApJS...69..831W) j: Caswell et al. (1995MNRAS.272...96C) k: Braz et al. (1990A&A...236..479B) l: MacLeod & Gaylard (1992MNRAS.256..519M) m: Schutte et al. (1993MNRAS.261..783S) n: van der Walt et al. (1995, Cat. <J/A+AS/110/81>) p: Caswell et al. (1995MNRAS.277..210C) q: Norris et al. (1987ApJ...321L.159N) r: Kemball et al. (1988ApJ...331L..37K) s: Ellingsen et al. (1996MNRAS.280..378E) t: Forster & Caswell (1989A&A...213..339F) u: Cesaroni et al. (1991A&A...252..278C) v: Palla et al. (1991A&A...246..249P) --- Ass4 Other association number=6 M: previous methanol maser detection O: previous OH maser detection W: previous water maser detection U: previous identification by a compact radio source N: sources discovered in this paper or reported in Walsh et al. (1995PASA...12..186W) x: non-detection in methanol emission by us --- r_Ass4 Source of Ass4 number=7 e: Henning et al. (1992A&AS...93..525H) f: Kurtz et al. (1994, Cat. <J/ApJS/91/659>) g: Churchwell (1990A&ARv...2...79C) h: Wood & Churchwell (1989ApJS...69..831W) j: Caswell et al. (1995MNRAS.272...96C) k: Braz et al. (1990A&A...236..479B) l: MacLeod & Gaylard (1992MNRAS.256..519M) m: Schutte et al. (1993MNRAS.261..783S) n: van der Walt et al. (1995, Cat. <J/A+AS/110/81>) p: Caswell et al. (1995MNRAS.277..210C) q: Norris et al. (1987ApJ...321L.159N) r: Kemball et al. (1988ApJ...331L..37K) s: Ellingsen et al. (1996MNRAS.280..378E) t: Forster & Caswell (1989A&A...213..339F) u: Cesaroni et al. (1991A&A...252..278C) v: Palla et al. (1991A&A...246..249P) --- tables.tex LaTeX version of the tables Patricia Bauer CDS 1997 Nov 14 Andrew Walsh <ajw@newt.phys.unsw.edu.au> J_MNRAS_291_261.xml The 7C(G) survey of radio sources at 151MHz - the Galactic plane at 80deg<l<104deg and 126deg<l<180deg, for |b|<5.5deg. J/MNRAS/294/607 J/MNRAS/294/607 7C The 7C(G) survey of radio sources at 151MHz - the Galactic plane at 80deg<l<104deg and 126deg<l<180deg, for |b|<5.5deg. S J Vessey D A Green Mon. Not. R. Astron. Soc. 294 607 1998 1998MNRAS.294..607V J/MNRAS/282/779 : 7C 151-MHz survey of region 9-16h 20-35deg (Waldram+ 1996) Radio sources Surveys catalogs radio continuum: general surveys Results form a survey of the northern Galactic plane (at declination >=30{deg} at 151MHz made with the Cambridge Low Frequency Synthesis Telescope are presented. This survey is designated 7C(G) - i.e. the Galactic portion of the ongoing 7C surveys. This covers the regions 80{deg}<l<104{deg} and 126{deg}<l<180{deg}, for |b|<=5.5{deg}, and has some coverage to |b|~9{deg}, with a resolution of ~70x70cosec{delta}arcsec^2^ (RAxDec). The observations, data reduction and calibration of this survey are described, and a catalogue of 6262 compact sources, with a completeness limit of ~0.25Jy over most of the survey region, is presented. The catalogue has an rms positional accuracy of better than 10arcsec, and the flux densities are tied to the scale of Roger, Bridle & Costain (1973AJ.....78.1030R) with an accuracy of better than 10 per cent.
7C(G) catalogue RAh Beam fitted position right ascension (B1950.0) number=1 The rms accuracies are 5arcsec in RA and 7arcsec in DE h RAm Beam fitted position right ascension (B1950.0) min RAs Beam fitted position right ascension (B1950.0) s DE- Beam fitted position declination sign --- DEd Beam fitted position declination (B1950.0) deg DEm Beam fitted position declination (B1950.0) arcmin DEs Beam fitted position declination (B1950.0) arcsec RA2h Centroid position right ascension (B1950.0) number=2 Multiple peaks integrated together have the same centroid position h RA2m Centroid position right ascension (B1950.0) min RA2s Centroid position right ascension (B1950.0) s DE2- Centroid position declination sign --- DE2d Centroid position declination (B1950.0) deg DE2m Centroid position declination (B1950.0) arcmin DE2s Centroid position declination (B1950.0) arcsec GLON Galactic longitude of the beam-fitted position deg GLAT Galactic latitude of the beam-fitted position deg S(bf) Beam fitted flux density number=3 Thew beam-fitted value is the preferred flux density unless the source is clearly extended, in which case the integrated flux density should be used. Jy S(in) Integrated flux density Jy S/N Signal-to-noise ratio --- Size Extent of the source size in units of the local beam area --- Peaks Number of individual peaks that where included in the flux integration --- n_Peaks The source is the main (M) or a component (C) peak in the integration --- Patricia Bauer CDS 1998 Apr 03 UNKNOWN UNKNOWN From MNRAS electronic version J_MNRAS_294_607.xml Statistical properties of HII regions in the disc of M100 J/MNRAS/297/255 J/MNRAS/297/255 HII region catalogue of M100 Statistical properties of HII regions in the disc of M100 J H Knapen Mon. Not. R. Astron. Soc. 297 255 1998 1998MNRAS.297..255K Galaxies, optical H II regions galaxies: individual (M 100) galaxies: ISM galaxies: spiral galaxies: structure HII regions From a new mosaic image in the H-{alpha} line of the complete disc of the spiral galaxy M100, a catalogue is composed listing 1948 individual HII regions. For each HII region, the catalogue gives its position relative to the centre of the galaxy, its deprojected distance to the centre, its radius, and its calibrated luminosity. An indication is included as to whether the HII region is located in the arms, between them, or in the circumnuclear star-forming region. The H-{alpha} image of M100 was obtained during two observing runs with the 4.2m WHT on La Palma, using the TAURUS camera in imaging mode. Since the field of view in this setup is limited by the filter size to around 5' diameter, four fields of the galaxy were imaged, two (eastern half of M100) during the night of 27 May 1991, and two (western half) during the night of 14 March 1992. Narrow band redshifted H-{alpha} filters with width of 15{AA} were used for the observations, centred at 6601{AA} for the H-{alpha} line observations (redshifted using the galaxy's systemic velocity of 1571km/s) and at 6577{AA} and 6565{AA} for the continuum. Exposure times were 1200 seconds for both the on-line and the continuum image on the first night, and 2x900 seconds on the second night. An EEV CCD chip was used during both observing runs, with a projected pixel size of 0.279arcsec, and a size of 1180x1280 pixels.
M100 NGC 4321 12 22 54.8 +15 49 20
The catalogue of HII regions in M100 ID identification number --- Xpos X position (toward East) from centre number=1 the centre is 2 20 22.9 +16 05 58 (B1950) arcsec Ypos Y position (toward North) from centre number=1 the centre is 2 20 22.9 +16 05 58 (B1950) arcsec Dist Deprojected distance from centre number=1 the centre is 2 20 22.9 +16 05 58 (B1950) arcsec PA Position angle wrt centre, N over E deg Radius Radius of HII region, in arcsec arcsec Flux Calibrated Flux in units of 10**36 erg/s 10+29W Location 0=interarm; 1=arm; 2=centre --- Francois Ochsenbein CDS 1998 Jul 21 Johan Knapen <knapen@star.herts.ac.uk> J_MNRAS_297_255.xml A radio survey of supersoft, persistent and transient X-ray sources in the Magellanic Cloud J/MNRAS/298/692 J/MNRAS/298/692 Radio Survey of X-ray sources A radio survey of supersoft, persistent and transient X-ray sources in the Magellanic Cloud R P Fender K A Southwell A K Tzioumis Mon. Not. R. Astron. Soc. 298 692 1998 1998MNRAS.298..692F Magellanic Clouds Radio lines X-ray sources binaries: general radio continuum: stars X-rays: stars We present a radio survey of X-ray sources in the Large and Small Magellanic clouds with the Australia Telescope Compact Array at 6.3 and 3.5 cm. Specifically, we have observed the fields of five LMC and two SMC supersoft X-ray sources, the X-ray binaries LMC X-1, X-2, X-3 & X-4, the X-ray transient Nova SMC 1992, and the soft gamma-ray repeater SGR 0525-66. None of the targets are detected as point sources at their catalogued positions. In particular, the proposed supersoft jet source RXJ 0513-69 is not detected, placing constraints on its radio luminosity compared to Galactic jet sources. Limits on emission from the black hole candidate systems LMC X-1 and X-3 are consistent with the radio behaviour of persistent Galactic black hole X-ray binaries, and a previous possible radio detection of LMC X-1 is found to almost certainly be due to nearby field sources. The SNR N49 in the field of SGR 0525-66 is mapped at higher resolution than previously, but there is still no evidence for any enhanced emission or disruption of the SNR at the location of the X-ray source. No radio point sources were detected at any wavelength at the catalogued locations of the target sources. In most cases a noise level of 50 microJy or so was achieved, making the 3-sigma upper limits very stringent indeed. The noise levels for LMC X-1 and SGR 0525-66 are considerably worse, due to their locations in radio-bright regions.
List of images with main characteristics FITSfile Name of FITS file (in subdirectory "fits") often we offset the pointing (commonly by +/- 10 arcsec in Dec) so do not assume target will lie exactly at centre of field, but instead check pointing centre. FITS headers give information on field and pixel size, and in HISTORY section, on reduction process (including phase calibration, CLEANing and the synthesised beam). Pixel values are Jy / beam ( = flux density for a point source). --- Frequency Observed frequency GHz RAh Right Ascension J2000 pointing centre (hours) h RAm Right Ascension J2000 (minutes) min RAs Right Ascension J2000 (seconds) s DE- Declination J2000 pointing centre (sign) --- DEd Declination J2000 (degrees) deg DEm Declination J2000 (minutes) arcmin DEs Declination J2000 (seconds) arcsec Npix Image size all images are squares made of square pixels, with Y-axis directed towards North. The images are stored in FITS format (floating-point pixel values). pix pixsize Pixel size arcsec Target Name of target --- Francois Ochsenbein CDS 1998 Jul 18 Robert P. Fender <rpf@astro.uva.nl> J_MNRAS_298_692.xml Mapping the {beta} Cephei instability strip: photometric variability of stars in the central part of the Cygnus OB2 association. J/MNRAS/298/753 J/MNRAS/298/753 Variables in Cygnus OB2 Mapping the {beta} Cephei instability strip: photometric variability of stars in the central part of the Cygnus OB2 association. A Pigulski Z Kolaczkowski Mon. Not. R. Astron. Soc. 298 753 1998 1998MNRAS.298..753P Associations, stellar Photometry, CCD Stars, B-type dust, extinction open clusters and associations: individual (Cyg OB2) stars: oscillations stars: variables: other We present the results of the photometric CCD search for B-type variables in the central region of the Cygnus OB2 association. We discover 29 new variables including two Beta Cephei stars. The photometric data in the Cousins I band are given in file photom.dat. In addition, we present BV(RI)c and H_{alpha}_ photometry for stars in the observed field. This is Table 4 of the paper, available only in electronic form.
Cross-identifications, positions, membership, BV(RI)c and H_alpha photometry of stars in the observed field CygON Star number according to Reddish et al. (1966PROE....5..111R), <Ass Cyg ON 2-NNNN> --- MT91 Star number according to Massey & Thompson (1991AJ....101.1408M), see Note number=1 The list of Massey & Thompson (1991AJ....101.1408M) contains 799 stars. These stars are labeled with 'MT'. All stars with numbers over 799 are new-designated ones extending above-mentioned numbering system. We label them with 'MTE'. --- Schulte Star number according to Schulte numbering system, see Note number=2 The details of Schulte's designation are explained in Section 3 of the paper. --- phFlag Flag set when photometry available in file photom.dat --- Xpos X coordinate of a star in Fig.2 pix Ypos Y coordinate of a star in Fig.2 pix Imag I magnitude, see Note number=3 For variable stars we use the following rules in listing their BV(RI)c magnitudes: for periodic variables we list the mean magnitude, while for the eclipsing binaries the magnitudes at the phase of maximum light are given. For the remaining variables we give the BV(RI)c magnitudes at one, arbitrarily chosen night, namely HJD 2450319. mag R-I R-I colour index, see Note number=3 For variable stars we use the following rules in listing their BV(RI)c magnitudes: for periodic variables we list the mean magnitude, while for the eclipsing binaries the magnitudes at the phase of maximum light are given. For the remaining variables we give the BV(RI)c magnitudes at one, arbitrarily chosen night, namely HJD 2450319. mag V-I V-I colour index, see Note number=3 For variable stars we use the following rules in listing their BV(RI)c magnitudes: for periodic variables we list the mean magnitude, while for the eclipsing binaries the magnitudes at the phase of maximum light are given. For the remaining variables we give the BV(RI)c magnitudes at one, arbitrarily chosen night, namely HJD 2450319. mag B-V B-V colour index, see Note number=3 For variable stars we use the following rules in listing their BV(RI)c magnitudes: for periodic variables we list the mean magnitude, while for the eclipsing binaries the magnitudes at the phase of maximum light are given. For the remaining variables we give the BV(RI)c magnitudes at one, arbitrarily chosen night, namely HJD 2450319. mag Alpha {alpha} colour index, see Note number=4 The definition of the alpha index we used is given by Pigulski et al. (1997AcA....47..365J). mag Memb Membershib flag, see text for explanation --- I0 Dereddened I magnitude mag (R-I)0 Dereddened R-I colour index mag RAh Right Ascension J2000 (hours) number=5 the positions were computed mainly from the GSC by Brian Skiff, Lowell Observatory (bas@lowell.Lowell.Edu) h RAm Right Ascension J2000 (minutes) number=5 the positions were computed mainly from the GSC by Brian Skiff, Lowell Observatory (bas@lowell.Lowell.Edu) min RAs Right Ascension J2000 (seconds) number=5 the positions were computed mainly from the GSC by Brian Skiff, Lowell Observatory (bas@lowell.Lowell.Edu) s DE- Declination J2000 (sign) number=5 the positions were computed mainly from the GSC by Brian Skiff, Lowell Observatory (bas@lowell.Lowell.Edu) --- DEd Declination J2000 (degrees) number=5 the positions were computed mainly from the GSC by Brian Skiff, Lowell Observatory (bas@lowell.Lowell.Edu) deg DEm Declination J2000 (minutes) number=5 the positions were computed mainly from the GSC by Brian Skiff, Lowell Observatory (bas@lowell.Lowell.Edu) arcmin DEs Declination J2000 (seconds) number=5 the positions were computed mainly from the GSC by Brian Skiff, Lowell Observatory (bas@lowell.Lowell.Edu) arcsec Differential Ic-filter photometry Name Star name --- HJD Heliocentric Julian day d DeltaI Differential Ic magnitudes mag Patricia Bauer CDS 1998 Aug 10 Andrzej Pigulski <pigulski@astro.uni.wroc.pl> Brian Skiff <bas@lowell.Lowell.Edu> for J2000 positions J_MNRAS_298_753.xml The Durham/UKST galaxy redshift survey - V. The catalogue. J/MNRAS/300/417 J/MNRAS/300/417 Durham/UKST Galaxy Redshift Survey The Durham/UKST galaxy redshift survey - V. The catalogue. A Ratcliffe T Shanks Q A Parker A Broadbent F G Watson A P Oates C A Collins R Fong Mon. Not. R. Astron. Soc. 300 417 1998 1998MNRAS.300..417R VII/203 : Las Campanas Redshift Survey (Shectman+ 1996) VII/175 : Edinburgh-Durham Southern Galaxy Clust. Cat. (Lumsden+ 1992) J/MNRAS/274/1071 : Edinburgh-Milano cluster redshift survey (Collins+ 1995) VII/193 : The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995) J/MNRAS/269/151 : APM cluster redshift survey. IV. (Dalton+, 1994) J/ApJS/107/201 : The Stromlo-APM Redshift Survey. IV. (Loveday+ 1996) Ratcliffe et al., Paper I. 1996MNRAS.281L..47R Ratcliffe et al., Paper II. 1998MNRAS.293..197R Ratcliffe et al., Paper III. 1998MNRAS.296..173R Ratcliffe et al., Paper IV. 1998MNRAS.296..191R Galaxy catalogs Radial velocities Redshifts catalogs cosmology: observations galaxies: clusters: general galaxies: distances and redshifts galaxies: general large-scale structure of universe We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.
Catalogue of the Durham/UKST Galaxy Redshift Survey DUGRS Galaxy designation --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign (1950) --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec bjmag b_j_ magnitude from the Edinburgh/Durham Sourthern Galaxy Catalog (Cat. <VII/175>) mag RV Radial velocity km/s Patricia Bauer CDS 1998 Dec 14 Tom Shanks <Tom.Shanks@durham.ac.uk> J_MNRAS_300_417.xml HST colour-magnitude diagrams of six old globular clusters in the LMC J/MNRAS/300/665 J/MNRAS/300/665 HST VI Photometry of Six LMC Old Globular Clusters HST colour-magnitude diagrams of six old globular clusters in the LMC K A G Olsen P W Hodge M Mateo E W Olszewski R A Schommer N B Suntzeff A R Walker Mon. Not. R. Astron. Soc. 300 665 1998 1998MNRAS.300..665O Clusters, globular Magellanic Clouds Photometry The following tables contain the results of photometry performed on Hubble Space Telescope WFPC2 images of the Large Magellanic Cloud globular clusters NGC 1754, 1835, 1898, 1916, 2005, and 2019. The magnitudes reported here were measured from Planetary Camera F555W and F814W images using DoPHOT (Schechter, Mateo, & Saha 1993) and afterwards transformed to Johnson V/Kron-Cousins I using equation 9 of Holtzman et al. (1995b). We carried out photometry on both long (1500 sec combined in F555W, 1800 sec in F814W) and short (40 sec combined in F555W, 60 sec in F814W) exposures. Where the short exposure photometry produced smaller errors, we report those magnitudes in place of those measured from the long exposures. For each star, we give an integer identifier, its x and y pixel position as measured in the F555W PC image, its V and I magnitude, the photometric errors reported by DoPHOT, both the V and I DoPHOT object types (multiplied by 10 if the reported magnitude was measured in the short exposure frame), and a flag if the star was removed during our procedure for statistical field star subtraction. Summary of data reduction and assessment of photometric accuracy: Cosmic ray rejection, correction for the y-dependent CTE effect (Holtzman et al. 1995a), geometric distortion correction, and bad pixel flagging were applied to the images before performing photometry. For the photometry, we used version 2.5 of DoPHOT, modified by Eric Deutsch to handle floating-point images. We found that there were insufficient numbers of bright, isolated stars in the PC frames for producing aperture corrections. Aperture corrections as a function of position in the frame were instead derived using WFPC2 point spread functions kindly provided by Peter Stetson. As these artificially generated aperture corrections agree well with ones derived from isolated stars in the WF chips, we trust that they are reliable to better than 0.05 mag. In agreement with the report of Whitmore & Heyer (1997), we found an offset in mean magnitudes between the short- and long-exposure photometry. We corrected for this effect by adjusting the short-exposure magnitudes to match, on average, those of the long exposures. Finally, we merged the short- and long- exposure lists of photometry as described above and transformed the magnitudes from the WFPC2 system to Johnson V/Kron-Cousins I, applying the Holtzman et al. (1995b) zero points. Statistical field star subtraction was performed using color-magnitude diagrams of the field stars produced from the combined WF frames. Completeness and random and systematic errors in the photometry were extensively modelled through artificial star tests. Crowding causes the completeness to be a strong function of position in the frame, with detection being most difficult near the cluster centers. In addition, we found that crowding introduces systematic errors in the photometry, generally <0.05 mag, that depend on the V-I and V of the star. Fortunately, these errors are well-understood. However, unknown errors in the zero points may persist at the ~0.05 mag level.
HST NGC 1754 04 54 18.70 -70 26 32.1 NGC 1835 05 05 06.44 -69 24 14.5 NGC 1898 05 16 42.41 -69 39 24.6 NGC 1916 05 19 -69 27 NGC 2005 05 30 10.36 -69 45 09.0 NGC 2019 05 31 56.73 -70 09 33.3
NGC 1754 VI photometry Star Star ID --- X X pixel position from F555W PC image pix Y Y pixel position from F555W PC image pix V V magnitude mag SigV Error in V magnitude (DoPHOT) mag I I magnitude mag SigI Error in I magnitude (DoPHOT) mag Vtyp DoPHOT object type for V measurement Where short exposure photometry was used, object type has been multiplied by 10. Explanation of DoPHOT object types is given by Schechter, Mateo, & Saha (1993) --- Ityp DoPHOT object type for I measurement --- Sub y Indicates that star was removed during statistical subtraction procedure --- NGC 1835 VI photometry Star Star ID --- X X pixel position from F555W PC image pix Y Y pixel position from F555W PC image pix V V magnitude mag SigV Error in V magnitude (DoPHOT) mag I I magnitude mag SigI Error in I magnitude (DoPHOT) mag Vtyp DoPHOT object type for V measurement Where short exposure photometry was used, object type has been multiplied by 10. Explanation of DoPHOT object types is given by Schechter, Mateo, & Saha (1993) --- Ityp DoPHOT object type for I measurement --- Sub y indicates that star was removed during statistical subtraction procedure --- NGC 1898 VI photometry Star Star ID --- X X pixel position from F555W PC image pix Y Y pixel position from F555W PC image pix V V magnitude mag SigV Error in V magnitude (DoPHOT) mag I I magnitude mag SigI Error in I magnitude (DoPHOT) mag Vtyp DoPHOT object type for V measurement Where short exposure photometry was used, object type has been multiplied by 10. Explanation of DoPHOT object types is given by Schechter, Mateo, & Saha (1993) --- Ityp DoPHOT object type for I measurement --- Sub y indicates that star was removed during statistical subtraction procedure --- NGC 1916 VI photometry Star Star ID --- X X pixel position from F555W PC image pix Y Y pixel position from F555W PC image pix V V magnitude mag SigV Error in V magnitude (DoPHOT) mag I I magnitude mag SigI Error in I magnitude (DoPHOT) mag Vtyp DoPHOT object type for V measurement Where short exposure photometry was used, object type has been multiplied by 10. Explanation of DoPHOT object types is given by Schechter, Mateo, & Saha (1993) --- Ityp DoPHOT object type for I measurement --- NGC 2005 VI photometry Star Star ID --- X X pixel position from F555W PC image pix Y Y pixel position from F555W PC image pix V V magnitude mag SigV Error in V magnitude (DoPHOT) mag I I magnitude mag SigI Error in I magnitude (DoPHOT) mag Vtyp DoPHOT object type for V measurement Where short exposure photometry was used, object type has been multiplied by 10. Explanation of DoPHOT object types is given by Schechter, Mateo, & Saha (1993) --- Ityp DoPHOT object type for I measurement --- Sub y indicates that star was removed during statistical subtraction procedure --- NGC 2019 VI photometry Star Star ID --- X X pixel position from F555W PC image pix Y Y pixel position from F555W PC image pix V V magnitude mag SigV Error in V magnitude (DoPHOT) mag I I magnitude mag SigI Error in I magnitude (DoPHOT) mag Vtyp DoPHOT object type for V measurement Where short exposure photometry was used, object type has been multiplied by 10. Explanation of DoPHOT object types is given by Schechter, Mateo, & Saha (1993) --- Ityp DoPHOT object type for I measurement --- Sub y indicates that star was removed during statistical subtraction procedure --- Knut Olsen NOAO and James E. Gass ADC/SSDOO 1998 Dec 30 We thank Eric Deutsch for his modifications to DoPHOT which made it easier to use and Peter Stetson for providing us with his WFPC2 PSFs. This work was supported by STScI grant GO05916 to NBS. J_MNRAS_300_665.xml High resolution spectra of Very Low-Mass Stars J/MNRAS/301/1031 J/MNRAS/301/1031 High resolution spectra of VLM stars High resolution spectra of Very Low-Mass Stars C G Tinney I N Reid Mon. Not. R. Astron. Soc. 301 1031 1998 1998MNRAS.301.1031T Spectroscopy Stars, dwarfs Stars, late-type A high resolution optical spectral atlas for three very low-mass stars are provided, along with a high resolution observation of an atmospheric absorption calibrator. This is the data used to produce Figures 4-9 in the paper. These data were acquired with CASPEC on the ESO3.6m telescope. The FWHM resolution is 16km/s (eg. 0.043nm at 800nm), at a dispersion of 9km/s. Incomplete wavelength coverage produces inter-order gaps at wavelengths longer than 804.5nm.
VB 8 LHS 429 Gl 644 C (vb8.dat) 16 55 35.7 -08 23 36 LHS 2065 LP 666-9 (lhs2065.dat) 08 53 36 -03 29 30 LP 944-20 (lp944-20.dat) 03 39 34.6 -35 25 51 mu Col HR 1996 HD 38666 (mucol.dat) 05 45 59.9 -32 18 23
Spectrum for VB8 Spectrum for LHS2065 Spectrum for LP944-20 Lambda Central wavelength of the flux bin 0.1nm Fnu Data in interorder gaps has value 0.0 mJy Atmospheric Spectrum for Mu Columbae Lambda Central wavelength of the flux bin 0.1nm Fnu Data in interorder gaps has value 0.0 mJy which have been normalised to value 1.0 in the continuum of the atmospheric standard star --- C.G. Tinney AAO 1999 Feb 04 J_MNRAS_301_1031.xml Beta Pictoris: the variable CaII H & K absorptions 1994-1996 J/MNRAS/304/733 J/MNRAS/304/733 Beta Pictoris 1994-96 Beta Pictoris: the variable CaII H & K absorptions 1994-1996 O K L Petterson W Tobin Mon. Not. R. Astron. Soc. 304 733 1999 1999MNRAS.304..733P Spectroscopy Stars, variable circumstellar matter line: profiles stars: individual (beta Pic) We present high-resolution spectroscopy of the variable CaII H & K absorptions in the star Beta Pictoris. 313 spectra were obtained on 53 nights between 1994 November and 1996 December in order to characterize the lines' behaviour and to test the Falling Evaporating Bodies (FEB) scenario. Near-continuous absorption activity was seen, including blue-shifted features, one of which rivalled the strength of that reported in 1997 June by Crawford et al. (1998MNRAS.294L..31C). Redshifted features at ~5-20km/s were present until the end of 1995 and are evocative of a year-long stream of infalling bodies with typically 4-5 objects in the line of sight. At higher velocities, features were shorter lived and generally broader and shallower. These correlations also apply to blue-shifted features. On 1995 June 9 we detected a probably narrow, short-lived feature at a redshift of ~130km/s. The FEB models predict that the strength of the H line may exceed the K line value as a body tracks across the stellar disc, but we have no convincing observation of this, though we did observe some events where the H & K absorptions evolved differently.
beta Pic HD 39060 05 47 17.0 -51 04 04
*Gaussian fits to observed variable Ca II absorptions. HJD HJD of mid observation d Depth Relative depth of absorption --- e_Depth Formal uncertainty in relative depth number=2 Formal uncertainties are often felt to underestimate true uncertainties. See Section 3 of paper for discussion. --- Vabs Velocity of absorption with respect to central feature number=1 The zero point of the velocity scale is established only approximately. See Section 2 of paper for discussion. km/s e_Vabs Formal uncertainty in relative velocity number=2 Formal uncertainties are often felt to underestimate true uncertainties. See Section 3 of paper for discussion. km/s FWHM Full-Width at Half Maximum of absorption km/s e_FWHM Formal uncertainty in FWHM number=2 Formal uncertainties are often felt to underestimate true uncertainties. See Section 3 of paper for discussion. km/s Line "h" if CaII H, "k" if CaII K --- SoB "s" if single feature, "b" if blended --- Classif classification number=3 Quality classification of the measured CaII variable absorptions. g: for single feature: an absorption that (possibly) no more than slightly overlaps with another is well-fitted by a Gaussian profile for . for blended feature: an absorption that clearly overlaps with one-or-more others is well-fitted by a Gaussian profile. p: for single feature: an absorption that (possibly) no more than slightly overlaps with another is a poorer fit to a Gaussian profile, either because the spectrum is noisy or because the profile is obviously non-Gaussian. p: for blended feature: an absorption that clearly overlaps with one-or-more others is a poorer fit to a Gaussian profile, either because the spectrum is noisy or because the profile is obviously non-Gaussian. ud: `Uncertain Decomposition': the feature has been fitted by a single Gaussian profile, but the signal-to-noise is insufficient to determine whether multiple Gaussians would provide a better fit. --- CS_Affect c: measures affected by central feature number=4 c: The feature blends with the deep, narrow, stellar-velocity circumstellar absorption, which has probably significantly affected the Gaussian parameters of the fitted profile, particularly if the division by the reference circumstellar profile has been imperfect. cr: The fit parameters are probably affected by imperfect filtering of cosmic rays. e: Fit parameters have been estimated by eye. --- CR cr: measures affected by a cosmic ray number=4 c: The feature blends with the deep, narrow, stellar-velocity circumstellar absorption, which has probably significantly affected the Gaussian parameters of the fitted profile, particularly if the division by the reference circumstellar profile has been imperfect. cr: The fit parameters are probably affected by imperfect filtering of cosmic rays. e: Fit parameters have been estimated by eye. --- By_eye e: measures are by-eye estimates number=4 c: The feature blends with the deep, narrow, stellar-velocity circumstellar absorption, which has probably significantly affected the Gaussian parameters of the fitted profile, particularly if the division by the reference circumstellar profile has been imperfect. cr: The fit parameters are probably affected by imperfect filtering of cosmic rays. e: Fit parameters have been estimated by eye. --- Comment Other comments --- Spectra obtained on 19 Nov 1994 Spectra obtained on 21 Nov 1994 Spectra obtained on 22 Nov 1994 Spectra obtained on 23 Nov 1994 Spectra obtained on 24 Nov 1994 Spectra obtained on 26 Nov 1994 Spectra obtained on 27 Nov 1994 Spectra obtained on 19 Apr 1995 Spectra obtained on 01 Aug 1995 Spectra obtained on 18 Dec 1995 Spectra obtained on 19 Dec 1995 Spectra obtained on 27 Jul 1995 Spectra obtained on 28 Jul 1995 Spectra obtained on 29 Jul 1995 Spectra obtained on 30 Jul 1995 Spectra obtained on 31 Jul 1995 Spectra obtained on 09 Jun 1995 Spectra obtained on 11 Jun 1995 Spectra obtained on 16 Jun 1995 Spectra obtained on 19 Jun 1995 Spectra obtained on 20 Jun 1995 Spectra obtained on 24 May 1995 Spectra obtained on 25 May 1995 Spectra obtained on 03 Nov 1995 Spectra obtained on 06 Nov 1995 Spectra obtained on 07 Nov 1995 Spectra obtained on 09 Nov 1995 Spectra obtained on 11 Nov 1995 Spectra obtained on 12 Nov 1995 Spectra obtained on 13 Nov 1995 Spectra obtained on 14 Nov 1995 Spectra obtained on 06 Oct 1995 Spectra obtained on 08 Oct 1995 Spectra obtained on 10 Oct 1995 Spectra obtained on 07 Sep 1995 Spectra obtained on 08 Sep 1995 Spectra obtained on 09 Sep 1995 Spectra obtained on 10 Sep 1995 Spectra obtained on 11 Sep 1995 Spectra obtained on 13 Sep 1995 Spectra obtained on 10 Dec 1996 Spectra obtained on 11 Dec 1996 Spectra obtained on 12 Dec 1996 Spectra obtained on 13 Dec 1996 Spectra obtained on 15 Dec 1996 Spectra obtained on 16 Dec 1996 Spectra obtained on 18 Dec 1996 Spectra obtained on 19 Dec 1996 Spectra obtained on 21 Dec 1996 Spectra obtained on 09 Jan 1996 Spectra obtained on 20 Jul 1996 Spectra obtained on 22 Jul 1996 Spectra obtained on 23 Jul 1996 OBSDate UTC date of observation "year-mon-dy" "YYYY-MM-DD" OBStime UTC time of mid observation "hh:mm:ss" "h:m:s" Line "H" if CaII H, "K" if CaII K --- Exposure Exposure duration s airmass Weighted airmass of observation --- HRV Approximate heliocentric radial velocity number=1 The zero point of the velocity scale is established only approximately. See Section 2 of paper for discussion. km/s Flux Flux in arbitrary units number=2 Examine the corresponding PostScript figure to ascertain extent to which spectrum may be affected by cosmic ray strikes --- Reference spectra Line "H" if CaII H, "K" if CaII K --- RV Approximate radial velocity with respect to central absorption km/s Flux Flux in arbitrary units. --- table2.ps PostScript version table2 William Tobin Astron., Univ. Canterbury, New Zealand 1998 Nov 05 William Tobin <w.tobin@phys.canterbury.ac.nz> J_MNRAS_304_733.xml The peculiar motions of early-type galaxies in two distant regions - II. The spectroscopic data. J/MNRAS/305/259 J/MNRAS/305/259 EFAR galaxies redshifts & velocity dispersions The peculiar motions of early-type galaxies in two distant regions - II. The spectroscopic data. G Wegner M Colless R P Saglia R K McMahan Jr. R L Davies D Burstein G Baggley Mon. Not. R. Astron. Soc. 305 259 1999 1999MNRAS.305..259W VII/193 : The CfA Redshift Catalogue (ZCAT), Version June 1995 (Huchra+ 1995) Wegner et al., Paper I 1996ApJS..106....1W Saglia et al., Paper III 1997MNRAS.292..499S Saglia et al., Paper IV 1997ApJS..109...79S Coless et al., Paper V 1999MNRAS.303..813C Galaxies, spectra Redshifts Velocity dispersion galaxies: clusters: general galaxies: distances and redshifts galaxies: elliptical and lenticular, cD large-scale structure of universe surveys We present the spectroscopic data for the galaxies studied in the EFAR project, which is designed to measure the properties and peculiar motions of early-type galaxies in two distant regions. We have obtained 1319 spectra of 714 early-type galaxies over 33 observing runs on 10 different telescopes. We describe the observations and data reductions used to measure redshifts, velocity dispersions and the Mgb and Mg_2_ Lick linestrength indices. Detailed simulations and intercomparison of the large number of repeat observations lead to reliable error estimates for all quantities. The measurements from different observing runs are calibrated to a common zero-point or scale before being combined, yielding a total of 706 redshifts, 676 velocity dispersions, 676 Mgb linestrengths and 582 Mg_2_ linestrengths. The median estimated errors in the combined measurements are {Delta}cz=20km/s, {Delta}sigma/sigma=9.1%, {Delta}Mgb/Mgb=7.2% and {Delta}Mg_2_=0.015mag. Comparison of our measurements with published data sets shows no systematic errors in the redshifts or velocity dispersions, and only small zero-point corrections to bring our linestrengths on to the standard Lick system. We have assigned galaxies to physical clusters by examining the line-of-sight velocity distributions based on EFAR and ZCAT redshifts, together with the projected distributions on the sky. We derive mean redshifts and velocity dispersions for these clusters, which will be used in estimating distances and peculiar velocities and to test for trends in the galaxy population with cluster mass. The spectroscopic parameters presented here for 706 galaxies combine high-quality data, uniform reduction and measurement procedures, and detailed error analysis. They form the largest single set of velocity dispersions and linestrengths for early-type galaxies published to date.
Individual Spectroscopic Measurements GINRUNSEQ Observation identifier --- Name Galaxy name --- Tel Telescope used --- ObsDate Observation date "DD/MM/YY" Qual Quality parameter --- n_Qual *: emission-line object with emission features listed in Notes column --- S/N Signal-to-noise ratio --- cz Redshift km/s e_cz rms uncertainty on cz km/s sigma Velocity dispersion km/s e_sigma rms uncertainty on sigma km/s Mgb Mgb linestrength 0.1nm e_Mgb rms uncertainty on Mgb 0.1nm Mg2 Mg_2_ linestrength mag e_Mg2 rms uncertainty on Mg2 mag Notes Notes number=1 double: EFAR galaxy is double star: EFAR object is a star not a galaxy mis-ID: spectrum is for some galaxy other than the nominated EFAR object mis-ID*: spectrum is for a nearby star rather than the EFAR object Mgb at sky: object is at a redshift which puts Mgb on the 5577{AA} sky line number=number: notes the duplicated pairs in the EFAR sample (see Paper I (Wegner et al., 1996ApJS..106....1W); only the first of the two GINs is used) 'H{beta} abs' or `H{beta} abs, [OIII]' means the redshift is based on the H{beta} absorption feature (and [OIII] if present), as the spectrum stops short of Mgb no dispersion or Mgb index is given for these objects). The objects for which we have no spectrum have GINs: 7, 20, 29, 30, 34, 35, 55, 62, 64, 67, 82, 83, 91, 104, 121, 131, 133, 134, 161, 181, 191, 214, 225, 228, 231, 234, 256, 265, 309, 327, 391, 405, 407, 417, 434, 435, 442, 450, 451, 452, 458, 463, 464, 465, 470, 475, 477, 483, 484, 486, 494, 516, 520, 521, 522, 523, 526, 544, 551, 553, 567, 569, 570, 575, 576, 577, 587, 594, 597, 603, 605, 624, 625, 644, 671, 727, 760, 793, 798, 801, 901. --- Spectroscopic parameters for the EFAR galaxies GIN Galaxy identification number --- Name Galaxy name --- CAN Cluster assignment number --- Nsp Number of spectra --- Ncz Number of redshifts number=1 Only objects with useful measurements are included; hence the lowest quality class present in this table is Qual = D, and the seven galaxies with only Qual = E spectra (GINs 123, 284, 389, 448, 599, 637 and 679) are omitted. --- Nsigma Number of dispersions number=1 Only objects with useful measurements are included; hence the lowest quality class present in this table is Qual = D, and the seven galaxies with only Qual = E spectra (GINs 123, 284, 389, 448, 599, 637 and 679) are omitted. --- NMgb Number of Mgb linestrength number=1 Only objects with useful measurements are included; hence the lowest quality class present in this table is Qual = D, and the seven galaxies with only Qual = E spectra (GINs 123, 284, 389, 448, 599, 637 and 679) are omitted. --- NMg2 Number of Mg2 linestrength number=1 Only objects with useful measurements are included; hence the lowest quality class present in this table is Qual = D, and the seven galaxies with only Qual = E spectra (GINs 123, 284, 389, 448, 599, 637 and 679) are omitted. --- cz Redshift (combined estimate) km/s e_cz Redshift (total error) km/s dcz Redshift (weighted rms error) km/s sigma Velocity dispersion (combined estimate) km/s e_sigma Velocity dispersion (total error) km/s dsigma Velocity dispersion (weighted rms error) km/s Mgb Mgb linestrength (combined estimate) 0.1nm e_Mgb Mgb linestrength (total error) 0.1nm dMgb Mgb linestrength (weighted rms error) 0.1nm Mg2 Mg_2_ linestrength (combined estimate) mag e_Mg2 Mg_2_ linestrength (total error) mag dMg2 Mg_2_ linestrength (weighted rms error) mag S/N Combined signal-to-noise ratio --- Qual Overall quality parameter number=1 Only objects with useful measurements are included; hence the lowest quality class present in this table is Qual = D, and the seven galaxies with only Qual = E spectra (GINs 123, 284, 389, 448, 599, 637 and 679) are omitted. --- n_Qual *: when galaxies possess emission lines --- Cluster mean redshifts and velocity dispersions CAN Cluster assignment number --- N1 Number of EFAR galaxies --- <cz>1 EFAR average redshift km/s e_<cz>1 rms uncertainty on <cz>1 km/s sigma1 EFAR velocity dispersion km/s N2 Number of EFAR+ZCAT galaxies --- <cz>2 EFAR+ZCAT average redshift km/s e_<cz>2 rms uncertainty on <cz>2 km/s sigma2 EFAR+ZCAT velocity dispersion km/s tables.tex LaTeX version of tables 3 & 5 James Marcout, Patricia Bauer CDS 1999 Aug 02 Matthew Colless <colless@mso.anu.edu.au> J_MNRAS_305_259.xml Faint UBVRI CCD sequences for wide-field surveys. II. UBVR sequences at {delta}=-30{deg} J/MNRAS/306/592 J/MNRAS/306/592 UBVR CCD sequences for wide-field surveys. II. Faint UBVRI CCD sequences for wide-field surveys. II. UBVR sequences at {delta}=-30{deg} S M Croom A Ratcliffe Q A Parker T Shanks B J Boyle R J Smith Mon. Not. R. Astron. Soc. 306 592 1999 1999MNRAS.306..592C J/MNRAS/276/33 : UBVRI CCD sequences for wide-field surveys. I. (Boyle+ 1995) Photometry, UBVRI Surveys techniques: photometric catalogues We present results from a continuing campaign to secure deep multi-colour CCD sequences for photoelectric calibration in UK Schmidt fields with galactic latitudes |b|>50{deg}. In this paper, we present UBVR photometry in 12 fields and BR photometry in a further 14 fields observed within UK Schmidt survey fields centered at {delta}=-30{deg}. Our observations were carried out with the 0.9m Telecope at the Cerro-Tololo Inter-American Observatory.
UBVR photometry Object Object designation (fNNNN-NNN) --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Bmag B magnitude mag e_Bmag rms uncertainty on Bmag mag B25mag B 25 pixel aperture magnitude number=1 25 pixel aperture magnitudes give good estimates of total galaxy magnitude for galaxies with isophotal diameter less than 20". mag s/g Star galaxy separation parameter b_10_-b_6_ number=2 Generally, objects with b_10_-b_6_ < -0.2 will be galaxies, although this does vary somewhat from field to field, depending on the seeing in each observation. --- Umag U magnitude mag e_Umag rms uncertainty on Umag mag U25mag U 25 pixel aperture magnitude number=1 25 pixel aperture magnitudes give good estimates of total galaxy magnitude for galaxies with isophotal diameter less than 20". mag Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag V25mag V 25 pixel aperture magnitude number=1 25 pixel aperture magnitudes give good estimates of total galaxy magnitude for galaxies with isophotal diameter less than 20". mag Rmag R magnitude mag e_Rmag rms uncertainty on Rmag mag R25mag R 25 pixel aperture magnitude number=1 25 pixel aperture magnitudes give good estimates of total galaxy magnitude for galaxies with isophotal diameter less than 20". mag Patricia Bauer CDS 1999 Apr 21 UNKNOWN UNKNOWN Copied on 22-Apr-1999 at http://icstar5.ph.ic.ac.uk:80/~scroom/phot/photom.html J_MNRAS_306_592.xml Infrared spectroscopic variability of Cygnus X-3 in outburst and quiescence. J/MNRAS/308/473 J/MNRAS/308/473 Cygnus X-3 IR spectra Infrared spectroscopic variability of Cygnus X-3 in outburst and quiescence. R P Fender M M Hanson G G Pooley Mon. Not. R. Astron. Soc. 308 473 1999 1999MNRAS.308..473F Binaries, X-ray Spectra, infrared binaries: close stars: individual: (Cygnus X-3) circumstellar matter infrared: stars We present four epochs, A, B, C and D, of resolution ({lambda}/{delta}{lambda}) = 1200, 2.12 micron spectroscopy of the peculiar X-ray binary Cygnus X-3. About a half dozen spectra taken with resolution 900, and at 1.62 micron are also included. These data were obtained using the FSpec near-infrared spectrometer (Williams, D., Thompson, C.L., Rieke, G.H., Montgomery, E. 1993, Proc. SPIE 1308, 482) on the Multiple Mirror Telescope (MMT). The MMT is located at an elevation of 2600 m at the top of Mt. Hopkins in southern Arizona and is jointly operated by the Smithsonian Astrophysics Observatory and the University of Arizona. The spectra are stored as ascii files, listing wavelength in Angstroms and relative flux. Each file contains a five line header, giving the UT, Heliocentric Julian date and phase of the X-ray system at the start of the integration, followed by the data points. Additional information about the spectra can be obtained in the paper.
Cyg X-3 V1521 Cyg H 2030+407 20 32 26.6 +40 57 09
Description of Cyg X-3 ascii spectra File Spectrum file name in subdirectory sp --- OBSdate Start of exposure "DD/MM/YY" OBSh Observation time h --- --- OBSm Observation time min --- --- OBSs Observation time s HJD Heliocentric Julian date d Exp Exposures number=1 Exposures defined as offsets in slit x sampled spectra x integration time per spectrum in seconds --- Phase Phase number=2 Phases represents start of exposure, using ephemeris of Kitamoto et al. (1995PASJ...47..233K) --- Patricia Bauer CDS 1999 May 02 Margaret M. Hanson <hanson@physics.uc.edu> J_MNRAS_308_473.xml Optical Gravitational Lensing Experiment. The catalog of clusters in the Small Magellanic Cloud. J/other/AcA/48.175 J/other/AcA/48.175 OGLE SMC clusters Optical Gravitational Lensing Experiment. The catalog of clusters in the Small Magellanic Cloud. G Pietrzynski A Udalski M Kubiak M Szymanski P Wozniak K Zebrun Acta Astron. 48 175 1998 1998AcA....48..175P I/244 : OGLE General Catalog of Stars. I. (Szymanski+ 1996) II/213 : OGLE Galactic Bulge periodic variables (Udalski+ 1996) J/A+AS/112/407 : OGLE variables in Sculptor dwarf galaxy (Kaluzny+, 1995) J/A+AS/125/343 : OGLE RR Lyr stars in omega Cen (Kaluzny+ 1997) J/other/AcA/46.389 : OGLE miscellaneous variable stars (Olech 1996) J/other/AcA/48.147 : OGLE SMC BVI photometry (Udalski+ 1998) J/other/AcA/48.289 : OGLE-I long-period & non-periodic variables (Zebrun 1998) I/221 : The Magellanic Catalogue of Stars - MACS (Tucholke+ 1996) Clusters, open Magellanic Clouds Photometry, UBVRI atlases catalogs galaxies: clusters: general Magellanic Clouds We present the catalog of clusters found in the area of ~2.4 square degrees in the central region of the Small Magellanic Cloud. The catalog contains data for 238 clusters, 72 of them are new objects. For each cluster equatorial coordinates, radii, approximate number of members, cross-identification, finding chart and color magnitude diagrams: V-(B-V) and V-(V-I) are provided.
SMC clusters OGLE-Cl SMC cluster designation (smcNNNN) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec Class Information about stellar density of the cluster relative to the background number=1 c: certain d: doubtful p: probable vp: very probable --- Rad Radius arcsec Rcore Core radius arcsec Nmemb Number of cluster members --- ID Cross identification number=2 K: Kron 1956PASP...68..125K L: Lindsay 1958MNRAS.118..172L L61: Lindsay 1961AJ.....66..169L HW: Hodge and Wright 1974AJ.....79..858H B: Brueck 1976ORROE...1....1B H86: Hodge 1986PASP...98.1113H BS: Bica and Smith 1995, Cat. <J/ApJS/101/41> OGLE: this paper --- SMC cluster candidates OGLE-Cl SMC cluster candidate designation (smcNNNN) --- RAh Right ascension (J2000) h RAm Right ascension (J2000) min RAs Right ascension (J2000) s DE- Declination sign --- DEd Declination (J2000) deg DEm Declination (J2000) arcmin DEs Declination (J2000) arcsec R Radius of the region arcsec Nmemb Number of members of the region --- ID Cross identification number=1 K: Kron 1956PASP...68..125K L: Lindsay 1958MNRAS.118..172L L61: Lindsay 1961AJ.....66..169L HW: Hodge and Wright 1974AJ.....79..858H B: Brueck 1976ORROE...1....1B H86: Hodge 1986PASP...98.1113H BS: Bica and Smith 1995, Cat. <J/ApJS/101/41> OGLE: this paper --- BVI photometry OGLE-Cl Cluster designation (smcNNNN) --- SMC-Cln Number of the star in the field --- Vmag V magnitude mag B-V B-V colour index mag V-I V-I colour index mag e_Bmag rms uncertainty on Bmag mag e_Vmag rms uncertainty on Vmag mag e_Imag rms uncertainty in Imag mag James Marcout, Patricia Bauer CDS 1998 Nov 19 UNKNOWN UNKNOWN Copied the 19 Nov 1998 from http://www.astrouw.edu.pl/~ftp/ogle/ogle2/clusters/smc/ J_other_AcA_48.175.xml The All Sky Automated Survey. The catalogue of the periodic variables stars in the Selected Fields. J/other/AcA/48.35 J/other/AcA/48.35 All Sky Automated Survey variable stars The All Sky Automated Survey. The catalogue of the periodic variables stars in the Selected Fields. G Pojmanski Acta Astron. 48 35 1998 1998AcA....48...35P http://www.astrouw.edu.pl/~gp/asas/asas.html : The All Sky Automated Survey Photometry Stars, variable Surveys catalogs stars: variables: general surveys Results of the first two months of observations using the All Sky Survey prototype camera are presented. More than 45000 stars in 24 Selected Fields covering 140 square degrees were monitored a few times per night resulting in the I-band catalog containing 10^7^ individual measurements. Period search revealed 126 variable stars brighter than 13mag with periods less than 20d. Only 30 of them are known variable stars included in the General Catalogue of Variable Stars (<II/214>). The other 90 objects are newly detected variable stars - mainly eclipsing binaries (75%) and pulsating stars (17%). We estimate that completeness of the current catalogs of variable stars is smaller than 50% already for the stars brighter than 9mag. The catalog is accessible over the WWW: http://www.astrouw.edu.pl/~gp/asas/asas.html
Selected fields observed during the first two months of ASAS operation Field Field name --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Periodic variables in the selected fields ASAS ASAS variable stars designation The designation is based on J2000 position; the "134460-3019.2" name was changed to "134500-3019.2" --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Type Variability classification ACV: {alpha}^2^ CVn type CEP(B): Cepheid B type DCEP: Delta Cep type DCEPS: Delta Cep type DSCT: Delta Scuti type EA: Algol type EB: Eclipsing binary EW: W UMa type MISC: Miscellaneous RRab: RRab Lyrae type RRc: RRc Lyrae type --- Imax I magnitude at maximum brightness mag DImag Light curve amplitude mag T0 Epoch of minimum brightness (HJD) d Per Period d CrossId Identification The cross-identification of ASAS J114736-6310.4 and 114736-6322.7 are flagged with an '*', they have been corrected at CDS (see the "History" section below) --- Patricia Bauer CDS 1999 Jan 07 UNKNOWN UNKNOWN * 15-Jun-1998 Copied from http://www.astrouw.edu.pl/~gp/asas/asas.html * 14-Jan-1999 Corrected the CKS identifications for 114736-6310.4 and 114736-6322.7, after discussion with Grzegorz Pojmanski: "I misplaced "OtherID" for the two adjacent lines (in Table 3)" and therefore the cross-identifications are: ASAS J114736-6310.4 = CKS91 11451-6253 ASAS J114736-6322.7 = CKS91 11451-6305 = HD 309036 J_other_AcA_48.35.xml Stars with ISM polarization observed with HPOL J/other/AcA/49.59 J/other/AcA/49.59 ISM polarization with HPOL Stars with ISM polarization observed with HPOL A J Weitenbeck Acta Astron. 49 59 1999 1999AcA....49...59W Polarization (ISM): dust, polarization Polarization data are given for stars whose polarizations are mostly interstellar which were observed for various programs with the University of Wisconsin spectropolarimeter (HPOL) during 1989-1994.
Polarization at V Star Star name --- Q Q parameter % U U parameter % e_Q rms uncertainty on Q and U % Pol Polarisation % PA Position angle deg Serkowski Law (WLR Version) Fit Parameters Star Star name --- lambdaMax Maximum wavelength 0.1nm e_lambdaMax rms uncertainty on lambdaMax 0.1nm Pmax Maximum polarisation % e_Pmax rms uncertainty on Pmax % PA Position angle deg e_PA rms uncertainty on PA deg K K parameter --- e_K rms uncertainty on K --- Polarization in other bands Star Star name --- Band Photometric band --- Q Q parameter % U U parameter % e_Q rms uncertainty on Q and U % Pol Polarisation % PA Position angle deg Individual notes Star Star name --- Note Text of the note --- Patricia Bauer CDS 1999 Aug 13 Anthony J. Weitenbeck <ajw@sal.wisc.edu> UNKNOWN UNKNOWN //www.sal.wisc.edu/~ajw/actast49.txt J_other_AcA_49.59.xml Photometric survey near the main Galactic meridian: 1. Photoelectric stellar magnitudes and colours in the UBVR system J/other/AN/316.225 J/other/AN/316.225 UBVR photoelectric survey Photometric survey near the main Galactic meridian: 1. Photoelectric stellar magnitudes and colours in the UBVR system V Andruk N Kharchenko E Schilbach R -D Scholz Astron. Nachr. 316 225 1995 1995AN....316..225A Photometry, UBVRI stars: colors UBVR system photoelectric photometry stellar magnitudes A catalogue of photoelectric stellar magnitudes and colours in the UBVR Johnson system in 47 sky areas with galaxies near the Main Galactic Meridian is presented. The catalogue includes 1141 stars within the V magnitude interval 4.5-15.5mag. The rms errors are +/-0.014, +/-0.026, +/-0.012, +/-0.016mag for stellar magnitudes V and colours (U-B), (B-V), (V-R), respectively. The catalogue contains accurate equatorial coordinates (alpha, delta)_1950.0_, too.
Catalogue of 1141 stellar magnitudes and colours in the UBVR system AKS95 Sequential number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag U-B U-B colour index mag e_U-B rms uncertainty on U-B mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag V-R V-R colour index mag e_V-R rms uncertainty on V-R mag Nobs Number of observations of the star --- Nnight Number of nights of observation of the star --- James Marcout, Patricia Bauer CDS 1997 Jul 11 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_AN_316.225.xml Candidates for a southern extension of the Karachentsev catalogue of isolated pairs of galaxies J/other/ApL/30.1 J/other/ApL/30.1 Southern catalogue of isolated pairs extension Candidates for a southern extension of the Karachentsev catalogue of isolated pairs of galaxies L Reduzzi R Rampazzo Astrophys. Lett. 30 1 1995 1995ApL....30....1R VII/77 : Isolated pairs of galaxies catalogue (Karachentsev+ 1972) VII/115 : ESO-LV catalogue (Lauberts+ 1989) J/A+AS/110/371 : Sourthern binary galaxies. I. (Soares+, 1995) Galaxies, photometry Galaxy catalogs Redshifts The paper presents a sample of double galaxies selected from The Surface Photometry Catalog of the ESO-Uppsala Galaxies (Cat. <VII/115>) using the Karachentsev (1972: K72, Cat. <VII/77>) criteria. Considering the large and growing number of observing facilities in that hemisphere, the sample aims to supply investigators with targets as homogeneous as possible to those in the Northern Catalog of Isolated Pairs of Galaxies (K72) which have been studied in a large frequency range. The paper discusses the sample degree of completeness, separation and velocity distributions. First inferences are sketched from the morphological association of pair members and from the study of the Holmberg effect. Being the primary purpose of the paper to provide a tool to investigators, an Atlas of images for the 301 best candidates pairs obtained using the Digitized Sky Survey (The Digitized Sky Survey was produced at the Space Telescope Science Institute (ST ScI) under U.S. Government grant NAG W-2166) is given. The Atlas reports for each pair member the relevant data as obtained from the current literature.
Southern catalogue of isolated pairs candidates No Pair number --- ESO ESO-LV (Cat. <VII/115>) identification number --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Decliantion sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec a25 Diameter at {mu}=25mag/arcsec^2^ arcsec Bmag B magnitude mag B-R B-R colour index mag T T (Hubble stage) number=1 Mean numerical index of stage along the Hubble sequence in RC2 system --- cz Recession velocity km/s r_cz cz reference number=2 F: Data from Fairall & Jones (1991, Cat. <VII/142>) dC: Data from da Costa, 1994, Priv. comm. --- Cat Category number=3 Some of the galaxies in the field around above pairs are not in the ESO-LV catalog because their diameter is lower than 1 arcmin. Further, in a few cases, a single object (or what appears as a single object) has two distinct entries in the catalog. Inspecting the fields, using the Digitized Sky Survey, we classified such pairs in the following way: PG = possible group PT = possible triplet S = single disturbed OP = optical pair NO = object that we reject after inspection essentially because in high density field --- Sep Distance between components arcsec Ntot Projected surface density --- Crit Criteria number=4 + : Strengh of the K72 criteria satisfied by the pair - : Strengh of the K72 criteria not satisfied by the pair --- James Marcout, Patricia Bauer CDS 1997 Apr 07 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_ApL_30.1.xml Galactic radio sources. II. High resolution 408 MHz observations J/other/AuJPA/14.77 J/other/AuJPA/14.77 408MHz galactic radio sources Galactic radio sources. II. High resolution 408 MHz observations P A Shaver W M Goss Australian J. Phys. Astrophys. Suppl. 14 77 1970 1970AuJPA..14...77S Radio sources Contour maps of 58 regions are presented showing 408 MHZ radioisophotes for over 200 galactic radio sources. Positions and integrated flux densities are listed for all the sources.
Source positions and integrated flux densities Source Galactic source designation --- n_Source Note on Source number=1 * Galactic source number is different in Part I (Shaver & Goss, 1970AuJPA..14....1S) due to positional measuring error and/or real shifts in position with frequency. + G25.4-0.2 has often been mistakenly identified as W42 --- GLON Source peak galactic longitude deg GLAT Source peak galactic latitude deg RAh Source peak right ascension (1950) h RAm Source peak right ascension (1950) min RAs Source peak right ascension (1950) s DE- Source peak declination sign (1950) --- DEd Source peak declination (1950) deg DEm Source peak declination (1950) arcmin DEs Source peak declination (1950) arcsec n_Tb Groups designation number=2 For a group, same n_Tb, from a to ag, the values Tb, S, Tbc, Sc, Fig and Name concern those of the group. They are repeated in each line of the group members. --- Tb Individual base brightness temperature K S408MHz Individual flux density at 408MHz Jy n_Tbc Groups designation number=3 For a group, same n_Tbc, the values Tbc, Sc, Fig and Name concern those of the group. They are repeated in each line of the group members. --- Tbc Composite base brightness temperature K S408MHzc Composite flux density at 408MHz Jy Fig Countour map in which the source appears --- Name Other names --- James Marcout, Patricia Bauer CDS 1999 Jan 18 UNKNOWN UNKNOWN Prepared via OCR at CDS, and proof-read by H. Andernach J_other_AuJPA_14.77.xml A new list of effective temperatures of chemically peculiar stars. II. J/other/BSAO/38.152 J/other/BSAO/38.152 Effective temperatures of CP stars A new list of effective temperatures of chemically peculiar stars. II. Yu V Glagolevskij Bull. Special Astrophys. Obs. 38 152 1994 1994BSAO...38..152G Effective temperatures Photometry Stars, peculiar A new list is presented of effective temperatures estimated for about 700 chemically peculiar stars from the photometric parameters, calibrated with the temperatures determined by Shallis Blackwell (Blackwell et al., 1980A&A....82..249B) method from the total flux of the energy emitted by the stars.
Dependence of parameters Q and X upon the effective temperatures Teff Effective temperature number=1 Construction of these dependences is based on the papers of Megessier (1988A&AS...72..551M), Stepien and Dominiczak (1989A&A...219..197S), Lamers (1981ApJ...245..593L), Shallis et al. (1985MNRAS.213..307S) and Glushneva (1987AZh....64..601G). K Q Q parameter number=2 Q parameter: reddening free index. See Johnson et al., 1953ApJ...117..313J X parameter: parameter of multicolour photometry --- X X parameter number=2 Q parameter: reddening free index. See Johnson et al., 1953ApJ...117..313J X parameter: parameter of multicolour photometry --- Effective temperatures of chemically peculiar stars HD HD number --- m_HD Multiplicity index on HD --- BD BD or CPD number --- Teff(Q) Effective temperature from parameter Q K u_Teff(Q) Uncertainty flag on Teff(Q) --- Teff(X) Effective temperature from parameter X of multicolour photometry K Teff(M) Effective temperature from total flux in Megessier (1988A&AS...72..551M) K n_Teff(M) Note on Teff(M) number=1 +: temperatures averaged from T(2100), T(u-b) and T(B2-G) *: temperature estimated for CP stars T<10500K from (B2-G) photometry --- Teff(SD) Effective temperature from Stepien and Dominiczak (1989A&A...219..197S) K Teff(L) Effective temperature from Lanz (1985A&A...144..191L) K Teff(Sh) Effective temperature from Shallis et al. (1985MNRAS.213..307S)x; K Teff(A) Effective temperature from Adelman's serie of papers K u_Teff(A) Uncertainty flag on Teff(A) --- Teff0 Average temperatures from Teff(Q), Teff(X), Teff(M), Teff(SD), Teff(L) and Teff(Sh) K u_Teff0 Uncertainty flag on Teff0 --- n_Teff0 Note number=2 Temperature marked by * estimated for CP stars T<10500K from (B2-G) photometry, the metallic-line stars (marked "m") have own calibration (B2-V1)-T_e_ (see the text and paper by Hauck & North, 1993A&A...269..403H). --- DeltaT Deviation of individual T from the average values T % James Marcout, Patricia Bauer CDS 1998 Aug 25 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_BSAO_38.152.xml Spectra of radio sources of the program "Cold" at the RATAN-600 radiotelescope J/other/BSAO/40.128 J/other/BSAO/40.128 RATAN-600 radio sources spectra Spectra of radio sources of the program "Cold" at the RATAN-600 radiotelescope N N Bursov Bull. Special Astrophys. Obs. 40 128 1996 1996BSAO...40..128B VIII/33 : Spectral characteristics of RATAN (RC) Catalog (Bursov+ 1989) J/A+AS/87/1 : RATAN-600 7.6 cm catalog of radio sources (Parijskij+ 1991) J/AZh/62/229 : Giant H II region Ratan-600 obs. (Berlin+ 1985) Radio sources Spectroscopy radio sources: catalog spectra In accordance with the program "Cold" in 1987-1988 and in 1996 deep surveys of the sky strip at the declination of the source SS 433 ({delta}~5{deg}+/-20') were made at the radio telescope RATAN-600. For the first time spectral characteristics of 400 sources from the RC catalog have been determined using only the data obtained with the RATAN-600. The maximum of the flux density distributions at the central wavelength {lambda}7.6cm is ~30mJy. The lower flux limit in the sample of the sources at the wavelengths 3.9, 7.6, 13.0, 31.0cm is 16, 9, 37, 61mJy, respectively. Spectra of 112 sources (28%) have been obtained for the first time, spectra of 90 (23%) sources have been made more accurate. For the first time the fluxes at the wavelengths 2.7, 3.9, 13.0 and 31.0cm (90% of data) have been measured. The maximum of the distribution of spectral indices for the entire sample of sources in the interval {lambda}{lambda}7.6-31.0cm falls at {alpha}=-0.86+/-0.04 (S_{nu}_{prop.to}{nu}^alpha^). About 20 (5%) sources of the sample have a maximum of radiation at a frequency of about 1GHz (GHz-Peaked-Spectrum radio sources), about 40 (10%) have a low-frequency cut off of the spectrum. About 70 (19%) sources have flat spectra ({alpha}>-0.5), 64 (18%) very steep ({alpha}<-1.1) spectra.
Flux densities of RC catalog radio sources Seq Sequential number --- RC Name of the source in the RC catalogue derived from the coordinates for the epoch J2000 --- n_RC Note on the sources number=1 n: sources with the spectra obtained for the first time c: sources with revised or corrected spectra For the rest of the sources, spectra was added --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec Dh Elevation drift of the source from the centre of the beam of the radiotelescope arcsec S2.7cm Flux density at {lambda}2.7cm (11GHz) mJy n_S2.7cm n: Flux values is lacking --- e_S2.7cm rms uncertainty on S2.7cm mJy l_S3.9cm Limit flag on S3.9cm --- S3.9cm Flux density at {lambda}3.9cm (7.69GHz) mJy n_S3.9cm n: Flux values is lacking --- e_S3.9cm rms uncertainty on S3.9cm mJy l_S7.6cm Limit flag on S7.6cm --- S7.6cm Flux density at {lambda}7.6cm (3.94GHz) mJy n_S7.6cm n: Flux values is lacking --- e_S7.6cm rms uncertainty on S7.6cm mJy l_S13.0cm Limit flag on S13.0cm --- S13.0cm Flux density at {lambda}13.0cm (2.3GHz) mJy n_S13.0cm n: Flux values is lacking --- e_S13.0cm rms uncertainty on S13.0cm mJy l_S31.0cm Limit flag on S31.0cm --- S31.0cm Flux density at {lambda}31.0cm (0.96GHz) mJy n_S31.0cm n: Flux values is lacking --- e_S31.0cm rms uncertainty on S31.0cm mJy SI Calculated spectral index in the wavelength interval {lambda}{lambda}76-31.0cm --- Spectrum Type of the source spectrum number=2 Types from the classification of Kellerman (1974, in, Galactic and Extragalactic Radio Astronomy, ed: G.L. Verschuur and K.I. Kellerman, Springer-Verlag, berlin, Heildelberg, New-York, 320.). S: The straight power assigned to extended optically thin synchrotron radio sources. C-: The spectrum has a negative second derivative of the dependence logS-log{nu} and is more steep at the short wavelengths. Such spectra are also assigned to extended radio sources Cmax: The power spectrum (class S) or dual power spectrum (class C-) at short waves, but there is a sharp cut off at the long wavelengths. Such spectra are produced by compact optically thick sources. C+: The spectrum has positive curvature with a rise at the long or the short wavelengths. CPX: Complex spectra with one or more minima. The spectra are generally believed to be composed of two or more spectra of class Cmax plus, in some case, of class S. The spectra of this class are also assigned to compact optically thick objects. F: Flat spectra --- James Marcout, Patricia Bauer CDS 1998 Aug 25 UNKNOWN UNKNOWN Prepared via OCR at CDS. UNKNOWN UNKNOWN Almost the same source list has also been published in Astron. Zh. (1997AZh....74....1B = 1997ARep...41...35B). There is some overlap of the above source lists with the list published in Astron. Astrophys. Suppl. 101 by Bursov et al. "Radio Spectra of RATAN-600 RC catalog sources" (1993A&AS..101..447B) J_other_BSAO_40.128.xml Investigation of RATAN-600 RC radio sources J/other/BSAO/40.5 J/other/BSAO/40.5 RATAN-600 RC radio sources Investigation of RATAN-600 RC radio sources Yu N Parijskij W M Goss A I Kopylov N S Soboleva A V Temirova O V Verkhodanov O P Zhelenkova M N Naugolnaya Bull. Special Astrophys. Obs. 40 5 1996 1996BSAO...40....5P VIII/33 : Spectral characteristics of RATAN (RC) Catalog (Bursov+ 1989) J/A+AS/87/1 : RATAN-600 7.6cm catalog of radio sources (Parijskij+ 1991) J/AZh/62/229 : Giant H II region Ratan-600 obs. (Berlin+ 1985) J/other/BSAO/40.128 : RATAN-600 radio sources spectra (Bursov 1996) Galaxies, radio Morphology Radio sources cosmology: miscellaneous observations radio galaxies: general We use the RATAN-600 radio telescope for picking up the most distant objects in the Universe. As a first step, about 100 steep spectrum FRII radio galaxies (SS FRII RG) from the RATAN-600 RC catalog (Parijskij et al., 1991, Cat. <J/A+AS/87/1>; 1992A&AS...96..583P) were mapped by the VLA and identified with optical objects down to 24-25 R mag. All the VLA images and all the deep CCD images of the RC SS fields, collected up to now, are given. An updated list of calibrators with the known redshifts of the same SS FRII class RGs was compiled to estimate photometric redshifts, redshifts from angular size - redshift relations and by the radio "standard candle" method. The mean redshift of the RC SS FRII RG list happened to be greater than 2. BVRI photometry was made, and by standard model fittings we estimated "color" redshifts and the ages of stellar systems of the parent gE galaxies in 14 cases. Several objects were found in which active star formation began in the first billion years after the Big Bang. We believe that more than 10000 of such old active galaxies are available on the sky and all of them are in the range of present day optical and radio facilities.
Redshifts and ages of the RC radio galaxy subsample RC Radio galaxy name --- dt Appropriate age of star population for the best model fittings of the observed BVRI fluxes Gyr zcc Estimated redshift of the RG using Chambers-Charlott (1990ApJ...348L...1C) models for SED of gE --- zph Photometrical redshift --- zLAS Redshift estimated using the object radio size --- zsp Redshift estimated from the "spectral index-redshift" relation --- zmn Mean redshift of zph, zLAS, zcc and zsp --- zsf Redshift of the beginning of the last burst of star formation in the RG --- zg0 Redshift of the galaxy gas component formation --- Tcc zcc corresponding cosmic time of the radio source (for the flat Universe, H0=75km/s/Mpc) Gyr Tmn zmn corresponding cosmic time of the radio source Gyr Tsf zsf corresponding moment Gyr Tbh0 Time of beginning of the giant black hole formation in the galactic centre Gyr Tg0 zg0 corresponding cosmic time Gyr The list of RC sources having the VLA images RC RATAN-600 RC name --- m_RC Multiplicty index on RC --- f_RC Modification, see "History" section below --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Beam VLA beam size arcsec n_Beam x when two components --- Beam2 Second VLA beam size when two components arcsec Freq VLA central frequency MHz l_LAS Limit flag on LAS --- LAS Largest angular size of the source measured between peaks of components arcsec l_Size Limit flag on Size --- Size Angular size of the components of the source arcsec n_Size x when two components; ): uncertainty flag --- l_Size2 Limit flag on size2 --- Size2 Second value when two components arcsec nSize p: point source --- SFreqc Flux density of components at the VLA central frequency mJy l_SFreq Limit flag on SFreq --- SFreq Total flux density of the object at the VLA central frequency mJy Sint Expected one of the integrated spectrum of the source mJy l_S3.9GHz Limit flag on S3.9GHz --- S3.9GHz Extrapolated flux density of the object at 3.9GHz mJy SI Spectral index --- n_SI Note on SI number=1 -: interval (C): for 0103+0524 and 1521+0434 D: for 2113+0445 f: flat i: inv,fl --- SI2 When interval --- GLON Galactic longitude deg GLAT Galactic latitude deg mlim Limiting optical magnitude mag Note *: individual note exists in notes.dat file --- Morph Morphology number=2 P: point Df: diffuse CJ: core with jet C: core WC: weak core BC: bright core D: double T: triple M: multiple Ext: extended FRII: Fanaroff-Riley II type structure (1974MNRAS.167p..31F) *: Note in notes.dat file --- Individual notes to table2.dat RC RATAN-600 RC name --- m_RC Multiplicity index on RC --- Note Text of the note --- Results of optical identification of the RC catalog sources RC RATAN-600 RC name --- m_RC Multiplicity index on RC --- f_RC Modification, see "History" section below --- RAh Optical identification right ascension (1950.0) h RAm Optical identification right ascension (1950.0) min RAs Optical identification right ascension (1950.0) s DE- Declination sign --- DEd Optical identification declination (1950.0) deg DEm Optical identification declination (1950.0) arcmin DEs Optical identification declination (1950.0) arcsec l_Rmag Limit flag on Rmag --- Rmag Observed R magnitude mag n_Rmag *: magnitude estimates made using the E-plate of POSS --- l_Rabs Limit flag on Rabs --- Rabs Correction for absorption by the Galaxy dust in R-band estimated from Burstein and Heiles (1982, Cat. <J/AJ/87/1165>) mag l_Rmag0 Limit flag on Rmag0 --- Rmag0 R magnitude corrected for absorption in the Galaxy mag l_DRmag Limit flag on DRmag --- DRmag Difference between limiting optical magnitude and absorption corrected R-magnitude mag l_oRA Limit flag on oRA --- oRA Right ascension position difference of the optical candidate and centroid (or core) of the radio source arcsec l_oDE Limit flag on oDE --- oDE Declination position difference of the optical candidate and centroid (or core) of the radio source arcsec James Marcout, Patricia Bauer CDS 1999 Apr 15 Heinz Andernach <heinz@polaris.astro.ugto.mx> UNKNOWN UNKNOWN Prepared via OCR at CDS in October 1998. An electronic version of the preprint was also supplied by Oleg V. Verkhodanov to H. Andernach in December 1996. The following corrections by H. Andernach were inserted in the 15-Apr-1999 version: - Table 2: 1339+0445 changed to 1339+0455 1806+0527 doesn't seem to exist - Table 3: 0506+0558 changed to 0506+0508 1235+0452 changed to 1235+0453 1339+0445 changed to 1339+0455 J_other_BSAO_40.5.xml The catalogue of nearby stars metallicities. J/other/KFNT/12.20 J/other/KFNT/12.20 Nearby stars metallicities The catalogue of nearby stars metallicities. V A Zakhozhaj E F Shaparenko Kinematika Fiz. Nebesn. Tel. 12, part no 2 20 1996 1996KFNT...12b..20Z V/70 : Nearby Stars, Preliminary 3rd Version (Gliese+ 1991) Abundances, [Fe/H] MK spectral classification Stars, nearby The catalogue for nearby stars' metallicities has been compiled. The catalogue contains 558 values obtained from photometric UBV data
Catalogue of nearby stars metallicities GJ Star name from Cat. <V/70> --- SpType Spectral type --- plx Parallax arcsec D(U-B) {delta}(U-B) mag [Fe/H] Metallicity Sun n_[Fe/H] Note on [Fe/H] --- James Marcout, Patricia Bauer CDS 1997 Jun 17 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_KFNT_12.20.xml BVRI Photometry of Spectroscopic Binaries J/other/Obs/116.382 J/other/Obs/116.382 BVRI Photometry of Spectroscopic Binaries BVRI Photometry of Spectroscopic Binaries R Miller W Osborn The Observatory 116, page ??? ??? 1996 1996Obs...116..382M Binaries, spectroscopic Photometry, UBVRI binaries: spectroscopic photometry, BVRI stars Photometry BVRI photometry has been obtained for 82 of the spectroscopic binaries with orbits published in The Observatory by Griffin and his collaborators. The observations were obtained on nineteen nights during 1994-95. Given here are the star name, Griffin's paper number for the spectroscopic orbit, the abbreviated calendar date and heliocentric Julian Date (HJD) of the observation, the derived V, (B-V), (V-R)c, and (R-I)c values, and the phase in the spectroscopic orbit. The mean photometric values are listed in the final entry for each star. One night of poor quality, 950128, was given half weight in forming the means. The rms error of a single observation is about 0.025 mag. for all indices.
Measures of 82 stars RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEm Declination 2000 (minutes) arcmin DEs Declination 2000 (seconds) arcsec Star Star designation --- Ref Number of Griffin's paper giving orbit number=1 references for the papers are given in Observatory 116,382 --- Date Abbreviated calendar date number=2 the values are blank for the average photometric results "YYMMDD" HJD Heliocentic modified Julian date number=2 the values are blank for the average photometric results d Vmag V magnitude mag B-V (B-V) magnitude mag V-R Johnson-Cousins (V-R) magnitude mag V-I Johnson-Cousins (V-I) magnitude mag Phase Phase in spectroscopic orbit number=2 the values are blank for the average photometric results --- Wayne Osborn Central Michigan Univ. 1997 Sep 23 Wayne Osborn <osborn@dune.phy.cmich.edu> J_other_Obs_116.382.xml HI profiles in the bridge region of the Magellanic Clouds J/other/PASAu/6.471 J/other/PASAu/6.471 Magellanic Clouds bridge region HI profiles HI profiles in the bridge region of the Magellanic Clouds R X McGee L M Newton Proc. Astron. Soc. Australia 6 471-500 1986 1986PASAu...6..471M H I data Magellanic Clouds Radial velocities Two hundred and seventeen HI profiles at positions approximately 1degree apart in the bridge region between the Small and Large Magellanic Clouds have been observed with a 15' arc beam. Diagrams of all the profiles, lists of column densities and average radial velocities are given, together with details of the extensive Gaussian analysis needed to account for the components. It is shown that the bridge region is most complex. (a) Two radial velocity (1) groups, +214 and +238km/s, represent the actual HI bridge between the two galaxies. (b) Three other components, at mean radial velocities of +155, +177 and +195km/s are seen to be integral parts of the SMC, stretching east to RA~04h. (c) A further three components in groups at mean radial Velocities +253, +272 and +293km/s appear to be extensions of HI from the main body of the LMC. Nine sets of five closely spaced observations in the lower Magellanic Stream and in the bridge region at high sensitivity supply further information about the region.
Radial velocities and column densities for neutral hydrogen RAh Right ascension (1950) h RAm Right ascension (1950) min DE- Declination sign --- DEd Declination (1950) deg RV Total profile radial velocity number=1 Radial velocities referred to the Sun km/s NH Hydrogen column density from the whole profile 10+20cm-2 RV1 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s n_RV1 *: Low featureless 190+320; no fittings attempted. --- NH1 Gaussian hydrogen column density 10+19cm-2 RV2 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH2 Gaussian hydrogen column density 10+19cm-2 RV3 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH3 Gaussian hydrogen column density 10+19cm-2 RV4 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH4 Gaussian hydrogen column density 10+19cm-2 RV5 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH5 Gaussian hydrogen column density 10+19cm-2 RV6 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH6 Gaussian hydrogen column density 10+19cm-2 RV7 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH7 Gaussian hydrogen column density 10+19cm-2 RV8 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH8 Gaussian hydrogen column density 10+19cm-2 Gaussian components of H-line profiles of nine sets of five closely spaced positions RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec RV1 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH1 Gaussian hydrogen column density 10+19cm-2 RV2 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH2 Gaussian hydrogen column density 10+19cm-2 RV3 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH3 Gaussian hydrogen column density 10+19cm-2 RV4 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH4 Gaussian hydrogen column density 10+19cm-2 RV5 Gaussian radial velocity number=1 Radial velocities referred to the Sun km/s NH5 Gaussian hydrogen column density 10+19cm-2 Marie-Jose Wagner, Patricia Bauer CDS 1996 Sep 03 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_PASAu_6.471.xml Coordinates and cross-identification of flare stars in Pleiades J/other/PZ/23.141 J/other/PZ/23.141 Flare stars in Pleiades Coordinates and cross-identification of flare stars in Pleiades E V Kazarovets Perem. Zvezdy 23 141 1993 1993PZ.....23..141K II/139 : General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988) II/131 : Tonantzintla Pleiades Flare Stars (Haro+ 1982) Cross identifications Stars, flare Stars, variable A brief account is given of the problems in identifying newly discovered variable stars with already known ones. These problems are most acute in dense stellar fields, for instance, in the Pleiades. To arrive to a homogeneous coordinates system for variable stars in the Pleiades, the author has measured the coordinates for nearly 550 stars in the region centered on Alcyone. This has made it possible to obtain for the first time accurate coordinates for 165 flare stars; then, for 46 stars we have round significant errors in the published coordinates. A cross-identification table between the GCVS (Cat. <II/139>) and the catalogue of Haro et al. (1982, Cat. <II/131>) has been compiled.
Pleiades Melotte 22 M 45 03 47.0 +24 07
Star positions Seq Sequential number --- Name Star name --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec HzII Hz II number (Hertzsprung, 1947AnLei..19a...1H, See Cat. <I/90>) --- James Marcout, Patricia Bauer CDS 1997 May 12 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_PZ_23.141.xml Stromgren photometry of stars in Baade's Window. I. The data. J/other/RMxAA/32.143 J/other/RMxAA/32.143 uvby photometry in Baade's Window Stromgren photometry of stars in Baade's Window. I. The data. A Ruelas-Mayorga G Garcia-Ruiz Rev. Mex. Astron. Astrofis. 32 143 1996 1996RMxAA..32..143R J/A+AS/93/61 : IR Stellar Population in Baade's window (Ruelas-Mayorga+ 1992) J/A+AS/97/587 : JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993) Photometry, uvby Populations, stellar Galaxy: center Galaxy: stellar content Hertzsprung-Russell (HR diagram) techniques: photometric We have obtained uvby data of a sample of 232 stars in Baade's Window. These observations are presented along with the corresponding diagrams. For a description of the uvby photometric system, see e.g. <GCPD/04>
Photometric information for the observed stars in Baade Window (BW) RG96 Name --- RAh Right ascension (2000) number=1 The errors are +/-0.1s in RA and +/-1" in DE h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) number=1 The errors are +/-0.1s in RA and +/-1" in DE deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec vmag v magnitude number=2 The error in vmag is upper-bounded by +/-0.02 mag b-y b-y colour index number=3 The error in b-y, m1 & c1 are upper-bounded by +/-0.01 mag m1 m1 colour index number=3 The error in b-y, m1 & c1 are upper-bounded by +/-0.01 mag c1 c1 colour index number=3 The error in b-y, m1 & c1 are upper-bounded by +/-0.01 mag James Marcout, Patricia Bauer CDS 1997 Sep 12 UNKNOWN UNKNOWN Prepared via OCR at CDS. In the original version, BW 137 has for position: 18 09 11.8 -29 36 65 J_other_RMxAA_32.143.xml Positions and proper motions in the area of the open cluster NGC 129 J/other/RMxAA/33.83 J/other/RMxAA/33.83 NGC 129 positions and proper motions Positions and proper motions in the area of the open cluster NGC 129 J Stock J Stock Rev. Mex. Astron. Astrofis. 33 83 1997 1997RMxAA..33...83S I/146 : Positions and Proper Motions - North (Roeser+, 1988) Clusters, open Magnitudes Proper motions astrometry open clusters and associations: individual (NGC 129) Positions and magnitudes were derived for 537 stars in the area of the open cluster NGC 129. Combining these positions with data from the three other sources, proper motions could be derived for 86 stars.
Positions catalog No Sequential number --- RAh Right ascension Equinox=1950.0, Epoch 1981.70 h RAm Right ascension Equinox=1950.0, Epoch 1981.70 min RAs Right ascension Equinox=1950.0, Epoch 1981.70 s DE- Declination sign --- DEd Declination Equinox=1950.0, Epoch 1981.70 deg DEm Declination Equinox=1950.0, Epoch 1981.70 arcmin DEs Declination Equinox=1950.0, Epoch 1981.70 arcsec Vmag Average visual magnitude mag e_RAs rms uncertainty on RAs 0.1ms e_DEs rms uncertainty on DEs mas Nimage Number of measured images --- Positions and proper motions No Sequential number --- RAh Right ascension Equinox=1950.0, Epoch 1981.70 h RAm Right ascension Equinox=1950.0, Epoch 1981.70 min RAs Right ascension Equinox=1950.0, Epoch 1981.70 s e_RAs rms uncertainty on RAs s DE- Declination sign --- DEd Declination Equinox=1950.0, Epoch 1981.70 deg DEm Declination Equinox=1950.0, Epoch 1981.70 arcmin DEs Declination Equinox=1950.0, Epoch 1981.70 arcsec e_DEs rms uncertainty on DEs arcsec pmRA Proper motion in RA mas/yr e_pmRA rms uncertainty on RA mas/yr pmDE Proper motion in DE mas/yr e_pmDE rms uncertainty on DE mas/yr Weight Total weight --- Nepochs Number of epochs that had contributed to the final positions --- James Marcout, Patricia Bauer CDS 1998 Aug 24 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_RMxAA_33.83.xml UBVRI observations of stars in the Guide Star Photometric Catalogue J/other/SAAOC/14.11 J/other/SAAOC/14.11 UBVRI photometry of GSPC stars UBVRI observations of stars in the Guide Star Photometric Catalogue D Kilkenny J D Laing South Afr. Astron. Obs. Circ. 14 11 1990 1990SAAOC..14...11K II/143 : Guide Star Photometric Catalog, Updated Version 1 (Lasker+ 1988,1996) Photometry, UBVRI Photoelectric UBVRI observations are given for 336 stars brighter than 11.5mag from the Hubble Space Telescope Guide Star Photometric Catalogue (GSPC). Apart from a Declination-dependent effect in the V magnitudes there are no systematic differences between GSPC (Cat. <II/143>) and SAAO (Menzies et al., 1989SAAOC..13....1M) data which are significantly greater than differences between the Landolt and E-region standard systems. The Declination effect might be due to the occurrence of unusually high atmospheric extinction coefficients at CTIO following the eruption of the Mexican volcano, El Chichon.
Mean UBVRI data for GSPC stars GSPC Star designation from the GSPC --- Vmag V magnitude number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. mag n_Vmag Note on Vmag number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. --- (B-V) (B-V) colour index number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. mag n_(B-V) Note on (B-V) number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. --- (U-B) (U-B) colour index number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. mag n_(U-B) Note on (U-B) number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. --- (V-R) (V-R) colour index number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. mag n_(V-R) Note on (V-R) number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. --- (V-I) (V-I) colour index number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. mag n_(V-I) Note on (V-I) number=1 The following convention has been used, where D is the difference between two observations (or the total range in the few cases where n_Vmag > 2) D < 0.02 mag : three decimal places given (82%) 0.02 < D < 0.05 mag : two decimal places (13%) 0.05 < D < 0.10 mag : two decimal places with colon ( 3%) 0.10 < D < 0.20 mag : one decimal place with colon ( 1%) Where D > 0.2 mag, the data have been omitted; this has occurred mostly for (U-B) of faint red stars. A few stars have V magnitudes marked with a double colon indicating possible or probable variability. --- o_Vmag Number of UBVRI observations --- n_o_Vmag Note on o_Vmag number=2 * implies o_Vmag observations in V magnitude and o_Vmag + 1 observations in the colours (because on an occasional "marginal" night the magnitudes were rejected but the colours retained) --- DVmag Vmag_GSPC_ minus Vmag_SAAO_ number=3 As the GSPC data are only quoted to two decimal places, the D values are given to the nearest 0.005mag. 10-3mag u_DVmag Uncertainty flag on DVmag --- D(B-V) (B-V)_GSPC_ minus (B-V)_SAAO_ number=3 As the GSPC data are only quoted to two decimal places, the D values are given to the nearest 0.005mag. 10-3mag u_D(B-V) Uncertainty flag on D(B-V) --- James Marcout, Patricia Bauer CDS 1997 Mar 17 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_SAAOC_14.11.xml A Study of Reddened Luminous Stars in the Southern Milky Way I. uvby Photometry J/other/SAAOC/15.40 J/other/SAAOC/15.40 Southern reddened luminous stars. I. A Study of Reddened Luminous Stars in the Southern Milky Way I. uvby Photometry D Kilkenny D C B Whittet South Afr. Astron. Obs. Circ. 15 40 1993 1993SAAOC..15...40K J/other/SAAOC/15.53 : Paper II. H{beta} photometry (Kilkenny 1993) J/other/SAAOC/15.65 : Paper III. VRI photometry (Kilkenny+ 1993) J/other/SAAOC/15.73 : Paper IV. JHK photometry (Spencer Jones+ 1993) Photometry, uvby Stars, luminous Stroemgren uvby photometry has been obtained for 270 reddened and very reddened OB stars selected from the Stephenson & Sanduleak (1971) catalogue of Luminous Stars in the Southern Milky Way (LSS), Cat. <III/43>. Corrections have been applied to convert the data as closely as possible to the reddened O stars observed by Crawford (1975PASP...87..481C). Uncorrected and corrected data ar presented in Tables 1 and 3, respectively.
Initial uvby photometry of LSSMV stars LSS LSS (Cat. <III/43>) number --- Vmag V magnitude mag (b-y) (b-y) colour index mag (v-b) (v-b) colour index mag (u-b) (u-b) colour index mag m1 m1 colour index mag c1 c1 colour index mag n_(b-y) Number of observations in uvby --- e_Vmag rms uncertainty on Vmag 10-3mag e_(b-y) rms uncertainty on (b-y) 10-3mag e_(v-b) rms uncertainty on (v-b) 10-3mag e_(u-b) rms uncertainty on (u-b) 10-3mag e_m1 rms uncertainty on m1 10-3mag e_c1 rms uncertainty on c1 10-3mag Uncorrected SAA0 photometry of Crawford and Sterken stars Origin Origin C: Crawford (1975PASP...87..481C) S: Sterken (1977A&A....57..361S) --- Star Star name --- Vmag V magnitude mag (b-y) (b-y) colour index mag m1 m1 colour index mag c1 c1 colour index mag n_(b-y) Number of observations in uvby --- Hbeta Hbeta colour index mag n_Hbeta Number of observations in Hbeta --- LSS LSS (Cat. <III/43>) number --- Corrected uvby photometry of LSSMW stars LSS LSS (Cat. <III/43>) number --- Vmag V magnitude mag (b-y) (b-y) colour index mag (v-b) (v-b) colour index mag (u-b) (u-b) colour index mag m1 m1 colour index mag c1 c1 colour index mag Note Notes number=1 a: Large std. dev. in table1; variable or probable variable b: Large difference between V from uvby and from VRI (paper III) (Kilkenny et al., 1993SAAOC..15...65K) even after allowance for reddening effects on magnitudes; probably variable c: Large difference between V from uvby and V from Drilling (1991ApJS...76.1033D) even after allowance for reddening effects on magnitudes; probably variable d: Drilling (1991ApJS...76.1033D) lists as probable variable: V flagged with ':' f: Eclipsing binary (Kilkenny et al. 1991IBVS.3659....1K) g: Ectipsing binary (Kilkenny al. 1992IBVS.3801....1K) h: Faint star(s) nearby; excluded from aperture i: Faint star(s) nearby included in aperture J: obvious nebulosity on photographic plates; variable background could effect photometry k: Weak nebulosity on photographic plates --- James Marcout, Patricia Bauer CDS 1997 Mar 10 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_SAAOC_15.40.xml A Study of Reddened Luminous Stars in the Southem Milky Way III. VRI Photometry J/other/SAAOC/15.65 J/other/SAAOC/15.65 Southern reddened luminous stars. III. A Study of Reddened Luminous Stars in the Southem Milky Way III. VRI Photometry D Kilkenny F van Wyk F Marang J H Spencer Jones D C B Whittet South Afr. Astron. Obs. Circ. 15 65 1993 1993SAAOC..15...65K J/other/SAAOC/15.40 : Paper I. uvby photometry (kilkenny+ 1993) J/other/SAAOC/15.53 : Paper II. Hbeta, reddening & distances (kilkenny 1993) J/other/SAAOC/15.73 : Paper IV. JHK photometry (Spencer Jones+ 1993) Photometry, VRI Stars, luminous V(RI)C photometry has been obtained for 262 reddened and very reddened stars selected from the Stephenson & Sanduleak (1971, Cat. <III/43>) catalogue of Luminous Stars in the Southern Milky Way (LSS). This photometry, together with data from earlier papers in this series, is used to identify a number of probable variable stars.
VRI photometry of reddened LSSMW stars LSS LSS (Cat. <III/43>) number --- Vmag V magnitude mag (V-R) (V-R) colour index mag (V-I) (V-I) colour index mag n_Vmag Number of observations in VRI --- e_Vmag rms uncertainty on Vmag 10-3mag e_(V-R) rms uncertainty on (V-B) 10-3mag e_(V-I) rms uncertainty on (V-I) 10-3mag Probable LSSMW variables based on V-magnitude standard deviations and intercomparisons greater than 0.05 mag LSS LSS (Cat. <III/43>) number --- e_ymag Standard deviation in ymag mag e_Vmag Standard deviation in Vmag mag e_Dr Drilling (1991ApJS...76.1033D) label --- (V-y) VRI-uvby magnitude difference mag (Dr-y) Drilling-uvby magnitude difference mag (Dr-V) Drilling-VRI magnitude difference mag Hbeta Hbeta colour index only when Hbeta<2.50 mag PNV Probably non-variable number=1 Stars for which no evidence for variability is found in our photometry (uvby, BRI, Hbeta) but which have large difference Drilling-SAAO. Three of the objects are in fields which are crowded and/or contaminated with strong nebulosity so that misidentification or "background" effects are more probable than variability. --- Com Comments number=2 EB : Eclipsing binary EB? : Probable eclipsing binary --- James Marcout, Patricia Bauer CDS 1997 Mar 10 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_SAAOC_15.65.xml A Study of Reddened Luminolls Stars in the Southern Milky Way IV. JHK Photometry J/other/SAAOC/15.73 J/other/SAAOC/15.73 Southern reddened luminous stars. IV. A Study of Reddened Luminolls Stars in the Southern Milky Way IV. JHK Photometry J H Spencer Jones D C B Whittet L He South Afr. Astron. Obs. Circ. 15 73 1993 1993SAAOC..15...73S J/other/SAAOC/15.40 : Paper I. uvby photometry (kilkenny+ 1993) J/other/SAAOC/15.53 : Paper II. Hbeta, reddening & distances (kilkenny 1993) J/other/SAAOC/15.65 : Paper III. VRI photometry (kilkenny+ 1993) Photometry, infrared Stars, luminous Infrared JHK measurements are presented for 232 reddened and very reddened stars selected from the Stephenson & Sanduleak (1971, Cat. <III/43>) catalogue of Luminous Stars in the Southern Milky Way (LSS).
JHK photometry of reddened LSS stars LSS LSS (Cat. <III/43>) number --- m_LSS Multiplicity index on LSS --- Jmag J magnitude mag Hmag H magnitude mag Kmag K magnitude mag o_Jmag Number of observations in JHK bands --- e_Jmag rms uncertainty on Jmag mag e_Hmag rms uncertainty on Hmag mag e_Kmag rms uncertainty on Kmag mag Notes Notes number=1 a) Too faint at K b) Too faint at H, K c) Of the two stars, the western one appears to be (from the colours) a reddened early-type star, although the Eastern one is indicated in the Stephenson & Sanduleak (1971, Cat. <III/43>) charts. We have observed the Western star in previous papers. --- James Marcout, Patricia Bauer CDS 1997 Mar 10 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_SAAOC_15.73.xml UBV Photometry of HD Stars in the Fields of Selected Cataclysmic Variables J/other/SAAOC/15.78 J/other/SAAOC/15.78 UBV photometry of HD stars UBV Photometry of HD Stars in the Fields of Selected Cataclysmic Variables D Kilkenny P E Barrett F Marang F van Wyk G Roberts H Winkler South Afr. Astron. Obs. Circ. 15 78 1993 1993SAAOC..15...78K Photometry, UBV Photoelectric UBV photometry is presented for over 400 HD stars which lie within about a degree of selected cataclysmic variables. The data will be combined with polarimetry to determine the distances of the CVs.
UBV photometry of HD stars near cataclysmic variables CV Cataclysmic variable name --- HD Field star HD name --- u_HD Uncertainty flag on HD name --- Vmag V magnitude mag (B-V) (B-V) colour index mag (U-B) (U-B) colour index mag n_Vmag Number of observations in UBV bands --- e_Vmag rms uncertainty on Vmag mag e_(B-V) rms uncertainty on (B-V) mag e_(U-B) rms uncertainty on (U-B) mag Notes *: individual notes number=1 HD 89945 : Variable. Observed range in V~0.28mag; 5 observations. HD 112343 : Identification uncertain. The fainter star (V=10.166) is presumably the correct star (HD type G5) and the brighter star is probably CD -29 10021. HD 116997 : Possibly variable. Observed range in (U-B)~0.1mag; 2 observations. HD 118257 : Possibly variable. Observed range in V~0.05mag; 2 observations. HD 154001 : Possibly variable. Single observation in 1991 different by 0.1mag from mean of 4 observations in 1992. HD 154882 : Pobably variable. Observed range in V~0.1mag; 4 observations. HD 154936 : Pobably variable. Observed range in V~0.09mag; 6 observations. HD 165761 : Variable. Observed range in V~0.18mag; 4 observations. HD 174107 : = V603Aql ! Two observations with mean V=11.44 are clearly of the CV itself. The two observations at V=9.95 are presumably of the wrong object although there is no star of such brightness within several arc minutes of V603 Aql (Duerbeck, 1987SSRv...45....1D, p. 163) HD 186669 : Probably variable. Observed range in V~0.09mag; 2 observations. Listed as V3960 Sgr in the General Catalogue of Variable Stars (Kholopov et al., 1990, Cat. <II/139>) Type LB (M5/7) HD 197010 : Variable. Observed range in V~0.13mag; 7 observations. HD 197042 : Variable. Observed range in V~0.13mag; 7 observations. HD 216482 : Close pair. The brighter star is presumably HD 216482 (=BD -3 5524) and the fainter star is then BD -3 5525. --- James Marcout, Patricia Bauer CDS 1997 Mar 17 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_other_SAAOC_15.78.xml CCD Photometry of the old open cluster NGC 7142 J/PASP/103/536 J/PASP/103/536 CCD Photometry of the old open cluster NGC 7142 CCD Photometry of the old open cluster NGC 7142 G Crinklaw F D Talbert Publ. Astron. Soc. Pac. 103 536 1991 1991PASP..103..536C Galaxy: general open clusters and associations: individual (NGC 7142) photometry variable stars CCD B,V observations on the NGC 7142 (1950 position 21h44.7 +65d34') field reveal the presence of a single short-period variable star. The color-magnitude diagram of the field shows evidence for small-scale variable absorption across the face of the cluster. The age of NGC 7142 appears to be confirmed as intermediate between that of M67 and NGC 188, and a new distance-modulus is found to be (m-M)0 = 11.4 +/- 0.9
CCD Photometry Star Running number --- V Magnitude mag B-V Color index mag o_V Number of observations --- Francois Ochsenbein CDS 1994 Jan 17 Greg Crinklaw J_PASP_103_536.xml Photoelectric UBV photometry of northern stars from the HK objective-prism survey. II. J/PASP/103/973 J/PASP/103/973 Photoelectric UBV from HK survey. II. Photoelectric UBV photometry of northern stars from the HK objective-prism survey. II. S P Doidinis T C Beers Publ. Astron. Soc. Pac. 103 973 1991 1991PASP..103..973D J/ApJS/76/1001 : UBV photometry of HK survey stars J/PASP/102/1392 : UBV photometry from HK survey. I (Doinidis+ 1990) J/AJ/108/268 : HK survey emission-line candidates positions J/AJ/112/1188 : HK survey emission-line candidates (Beers+ 1996) Photometry, UBV HK objective prism survey northern stars UBV photometry Photoelectric UBV photometry is presented for a sample of 165 stars drawn from the extension of the HK objective-prism/interference-filter survey of Beers, Preston and Shectman (1985AJ.....90.2089B) to the northern galactic hemisphere. These results are part of continuing follow-up observations of candidate metal-deficient and horizontal-branch field stars and other interesting stars identified in the survey. A complete set of photometric observations is now available for three of the 25-square-degree survey fields. We estimate that the complete photometric sample of 299 northern HK candidates obtained to date contains on order 90 main-sequences turnoff, subgiant, and giant stars with [Fe/H]<=-1.0, 50 field blue horizontal-branch stars, and 30 stars with the photometric properties of field blue stragglers.
Photoelectric data for program stars BS Telescope identification. BS = Burrell Schmidt --- Npl Plate identification number --- Nstar Star identification number --- m_Nstar Multiplicity index on star identification --- RAh Right Ascension 1950.0 h RAm Right Ascension 1950.0 min RAs Right Ascension 1950.0 s DE- Declination sign --- DEd Declination 1950.0 deg DEm Declination 1950.0 arcmin DEs Declination 1950.0 arcsec GLON Galactic Longitude deg GLAT Galactic Latitude deg Vmag Observed V magnitude mag B-V Observed B-V color mag U-B Observed U-B color mag o_Vmag Number of observations included in V, B-V and U-B data --- E(B-V) Estimated reddening at plate center mag Class Classification of objective-prism spectrum code number=1 MP = Metal Poor A = A type spectrum B = B type spectrum C = Continuous spectrum AB = AB type spectrum E = Emission lines detected P = Peculiar Colons indicate uncertainty in the classification. Dual classifications indicate intermediate cases. --- Patrica Bauer CDS 1994 Jul 07 Timothy Beers <beers@msupa.pa.msu.edu> J_PASP_103_973.xml A BV Color-Magnitude Diagram for the Galactic Globular Cluster NGC 1851 J/PASP/104/1063 J/PASP/104/1063 BV Color-Magnitude Diagram for NGC 1851 A BV Color-Magnitude Diagram for the Galactic Globular Cluster NGC 1851 A R Walker Publ. Astron. Soc. Pac. 104 1063 1992 1992PASP..104.1063W J/AJ/105/527 : RR Lyr stars in NGC 1835 (Walker 1993) J/AJ/112/2020 : UBV Photometry of NGC 1841 (Alcaino+ 1996) Clusters, globular Photometry, CCD BV photometry is provided for 1,234 stars in the magnitude range 13-18 in an annulus between 5 and 20 arc seconds from the center of NGC 1851 and for 1,247 stars in the magnitude range 18-23 at a distance of more than 240 arc seconds from the center. For stars in the magnitude range 16-21, the errors in B-V increase with magnitude from 0.005 mag. to 0.022 mag. See the document file (walker.txt or walker.tex) by Nancy G. Roman for more details.
NGC 1851 C 0512-400 05 14 06.3 -40 02 50
Position & Photometry No Number --- X coordinate (0.478arcsec/pix toward North) pix Y coordinate (0.478arcsec/pix toward East) pix Vmag magnitude mag u_Vmag Uncertaintly flag (:) --- (B-V) color mag u_(B-V) Uncertaintly flag (:) --- Rem Remark --- walker.tex NSSDC-ADC document walker.txt NSSDC-ADC Description CDS 1993 Jul 16 J_PASP_104_1063.xml Improved CCD Standard Fields J/PASP/104/553 J/PASP/104/553 CCD Standard Fields Improved CCD Standard Fields S C Odewahn C Bryja R M Humphreys Publ. Astron. Soc. Pac. 104 553 1992 1992PASP..104..553O Photometry, CCD Stars, standard Multiple nights of CCD observations of NGC 7790, NGC 7006, and NGC 4147 are combined in order to establish a deep sequence of photometric standards whose errors have been objectively derived through statistical comparisons. In addition to extending these previously studied fields to a fainter limit, the range in observed color is increased making the mean sequences more suitable for deriving photometric transformation coefficients.
Tables 2, 3 and 4 (NGC 4147, 7006 and 7790) Name Cluster Name --- Star Star Number --- X (plate coordinate) pix Y (plate coordinate) pix V V magnitude mag e_V mean error (V) mag o_V Number of observations (V) --- (B-V) B-V mag e_(B-V) mean error (B-V) mag o_(B-V) Number of observations (B-V) --- (V-R) V-R mag e_(V-R) mean error (V-R) mag o_(V-R) Number of observations (V-R) --- odewahn.tex ADC Documentation (requires "adc.sty") CDS 1993 Jul 28 J_PASP_104_553.xml The Spectrum of the Planetary Nebula NGC 6567 J/PASP/105/1279 J/PASP/105/1279 The Spectrum of NGC 6567 The Spectrum of the Planetary Nebula NGC 6567 S Hyung L H Aller W A Feibelman PASP 105 1279 1993 1993PASP..105.1279H Abundances Nebulae Nonstellar objects Planetary nebulae Spectroscopy Tables are presented for 126 lines in the optical region of the planetary nebula, NGC 6567.
Optical region line intensities lamobs Observed wavelength 0.1nm lamlab Laboratory wavelength 0.1nm elem Elemnent --- mult Multiplet number --- ext *Extinction coefficient --- int *Intensity corrected for extinction Hbeta flux *Uncorrected flux Hbeta e_flux Formal root-mean-square error percent Nancy G. Roman NASA/NSSDC/ADC 1994 May 19 J_PASP_105_1279.xml Rotation Periods of Open Cluster Stars, II J/PASP/105/1407 J/PASP/105/1407 Rotation Periods of Open Cluster Stars II Rotation Periods of Open Cluster Stars, II C F Prosser M D Shetrone E Marilli S Catalano S D Williams D E Backman B D Laaksonen V Adige L A Marschall J R Stauffer Publ. Astron. Soc. Pac. 105 1407 1993 1993PASP..105.1407P J/PASP/105/269 : Light Curves for 10 Rapidly Rotating Stars (Prosser+, 1993) Prosser, C. 1992, AJ 103, 488 Radick, R. 1991, "The Sun in Time" van den Bergh S., ed. Sonnett, C., Giampapa, M., and Matthews, M. (University of Arizona), p. 787 Schussler, M., and Solanki, S. 1992, A&A 264, L13 Photometry Stars, physical properties Stars, variable This catalog contains the individual instrumental V magnitudes of 16 stars from a photometric monitoring program of 21 stars observed during 1992 in the Pleiades and Alpha Persei open clusters. The observations were undertaken in order to determine rotational periods of the stars from observed brightness variations. Brightness variations for an additional five cluster stars are also given. The magnitudes in this dataset are purely instrumental and have not been converted to a standard V mag system, nor have they been converted to correspond to the mean V mag of the target star. These magnitudes of the target and comparison stars should therefore only be used in a differential sense. (See note (3)). The column format varies slightly for each star listing because different observations were measured to different precision and different numbers of comparison stars were used. The general format is that the first column contains the target stars' magnitude, followed by two or more columns of comparison star magnitudes, and the Julian Dates of observation in the last column.
HII 314, Pleiades HII 708, Pleiades HII 727, Pleiades v relative V magnitude of target star mag N number of 20 sec observations in average --- JD Julian Date of observation d HII 2741, Pleiades mag relative V magnitude of target star mag v-A relative V magnitude of comparison star A mag v-C relative V magnitude of comparison star C mag JD Julian Date of observation d HII 2881, Pleiades HE 373, Alpha Persei HE 622 = AP 19, Alpha Persei AP 37, Alpha Persei AP 127, Alpha Persei AP 149, Alpha Persei AP 226, Alpha Persei AP 244, Alpha Persei (MDS obs.) AP 117, Alpha Persei mag relative V magnitude of target star mag v-A relative V magnitude of comparison star A mag v-A relative V magnitude of comparison star B mag v-B relative V magnitude of comparison star C mag JD Julian Date of observation d AP 63, Alpha Persei AP 86, Alpha Persei (NURO obs.) AP 117, Alpha Persei mag relative V magnitude of target star mag v-A relative V magnitude of comparison star A mag v-B relative V magnitude of comparison star B mag JD Julian Date of observation d AP 124, Alpha Persei mag relative V magnitude of target star mag v-A relative V magnitude of comparison star A mag v-B relative V magnitude of comparison star B mag JD Julian Date of observation d James Gass ADC 1996 Jul 31 UNKNOWN UNKNOWN July 1996: Original table separated by target star(s) by ADC (James Gass) July 1996: Documentation standardized at ADC (James Gass) J_PASP_105_1407.xml A Simple Description of Light Curves if W UMa Systems J/PASP/105/1433 J/PASP/105/1433 Light Curves of W UMa Systems A Simple Description of Light Curves if W UMa Systems S M Rucinski Publ. Astron. Soc. Pac. 105 1433 1993 1993PASP..105.1433R Binaries, contact Stars, variable Fourier cosine coefficients a(1) to a(6) are tabulated and shown graphically for light curves of contract binary stars of one (solar) effective temperature, with orbital inclinations (i), 30 deg.le.i.le.90deg., mass ratios (q), 0.05.le.q.le.1, and three values of the degree of contact, f=0, 0.5, 1. The coefficients, combined with additional tables of depths of minima, can be used for statistical estimates of ensemble properties of light curves of contact systems in stellar systems or for approximate determinations of orbital elements of individual contact binaries. Tables of all eleven coefficients a(0) to a(10) for all combinations of i and q are accessible using the ftp file-transfer mechanism.
There is a need for a simple method to obtain essential parameters for contact binaries without the necessity for full light-curve synthesis solutions. A statistical method is also required to determine the expected distribution of variability amplitudes with observations. Only one set of temperature is given: the solar case with T(eff)=5770 K, for photometric band V, with gravity darkening exponent beta=0.08 in T(eff) proportional to g to the beta and bolometric albedo A=0.5. Nevertheless. the calculations should be applicable to a large range of effective temperatures. Light curves depend practically only on three parameters, the mass ratio, q, the inclination, i, and the degree of contact, f. The observed light curve should be expressed in light units, relative to the maximum at phases 0.25 or 0.75. (If the maxima are unequal, use the higher maximum.) A very good representation of a light curve can be usually obtained by calculating the Fourier series l = sum (ai*cos(2*pi*i*phase) and then truncating the curved part of the secondary (occultation) eclipse at the level l(180) using the tables of b the depth of secondary minima, 1-l(180)).
Coefficients for f=0 (Inner Contact) Coefficients for f=0.5 Coefficients for f=1 (Outer Contact) i The inclination deg q The mass ratio --- a0 The coefficient, a(0) --- a1 The coefficient, a(1) --- a2 The coefficient, a(2) --- a3 The coefficient, a(3) --- a4 The coefficient, a(4) --- a5 The coefficient, a(5) --- a6 The coefficient, a(6) --- a7 The coefficient, a(7) --- a8 The coefficient, a(8) --- a9 The coefficient, a(8) --- a10 The coefficient, a(10) --- Depth of minimum for f=0 Depth of minimum for f=0.5 Depth of minimum for f=1 i The inclination deg c The mass ratio --- l0 Depth of minimum for eclipse of more massive component --- l180 Depth of minimum for eclipse of less massive component --- Nancy G. Roman ADC/SSDOO 1995 Sep 06 UNKNOWN UNKNOWN Each line contains the value of inclination (degr), mass-ratio, and two depths of minima 1-l(0) and 1-l(180) for eclipses of more- and less-massive components, respectively. The division into three parts according to the degree of contact is the same as for "coef" Note that a very good representation of a light curve can be usually obtained by calculating the Fourier series l = sum (ai*cos(2*pi*i*phase) and then truncating the curved part of the secondary (occultation) eclipse at the level l0 using the tables of the depth of secondary minima, l180. J_PASP_105_1433.xml Distant (r>5 kpc) OB Stars in the Galaxy J/PASP/105/1465 J/PASP/105/1465 Distant OB Stars in the Galaxy Distant (r>5 kpc) OB Stars in the Galaxy B C Reed Publ. Astron. Soc. Pacific 105 1465 1993 1993PASP..105.1465R Photometry, beta Photometry, UBV Stars, O Distances and reddenings have been computed from UBVbeta photometry for 1044 stars in the Stephenson and Sanduleak (1971) "Catalog of Luminous Stars in the Southern Milky Way".
Photometry and distances num LS number --- V V magnitude mag BV B-V color mag UB U-B color mag beta Beta color mag dist Distance from sun kpc ex B-V color excess mag glon Galactic longitude deg glat Galactic latitude deg nV Number of measurements of V --- nBV Number of measurements of B-V --- nUB Number of measurements of U-B --- x x coordinate of star in galactic plane kpc y y coordinate of star in galactic plane kpc N.G. Roman NASA, ADC 1995 Jan 20 J_PASP_105_1465.xml Photometric Light Curves for Ten Rapidly Rotating Stars in Alpha Persei, the Pleiades, and the Field J/PASP/105/269 J/PASP/105/269 Light Curves for 10 Rapidly Rotating Stars Photometric Light Curves for Ten Rapidly Rotating Stars in Alpha Persei, the Pleiades, and the Field C F Prosser R E Schild J R Stauffer B F Jones Publ. Astron. Soc. Pac. 105 269 1993 1993PASP..105..269P Photometry Rotational velocities Stars, variable This catalog contains photometric V magnitudes as a function of Julian Date for nine G and K type stars in the open clusters Alpha Persei and the Pleiades, and for a young field star, WTT 040012+2545. The observations were undertaken in order to determine rotational periods of the stars from observed brightness variations. The measurements have not been transformed to a photometric standard, but simultaneous magnitudes for comparison stars in the same CCD fields are included. Photometric accuracies of 1% or better are claimed. The observations were made in late 1991 as part of a program to determine rotational periods from observed brightness variations. Since the original data file contained records whose format varied from star to star, the ADC has split the data into separate files. The column format varies slightly for each star listing since different observations were made to different precision and different numbers of comparison stars were used. The general format is that the first column contains the target star's measured V magnitude, followed by two or more columns of comparison star magnitudes. The Julian Dates of observation are given in the last column. We present the results from a photometric monitoring program of 10 rapidly rotating stars observed during 1991 using the Fred Lawrence Whipple Observatory (FLWO) 48-inch telescope. Brightness variations for an additional six cluster stars observed with the Lick 40-inch telescope are also given. The periods and light curves for seven Alpha Persei members, two Pleiades members, and one naked T-Tauri field star are reported. The individual photometric measurements have been deposited with the NSSDC.
AP60, Alpha Persei AP86, Alpha Persei AP100, Alpha Persei HII1136, Pleiades WTT040012 +2545, field V V magnitude of target star mag V-A V magnitude of comparison star A mag V-B V magnitude of comparison star B mag JD Julian Date of observation d AP91, AP93 Alpha Persei ap91 V magnitude of star AP91 mag ap93 V magnitude of star AP93 mag V-A V magnitude of comparison star A mag V-B V magnitude of comparison star B mag V-C V magnitude of comparison star C mag JD Julian Date of observation d AP139, Alpha Persei AP258, Alpha Persei mag V magnitude of target star mag V-A V magnitude of comparison star A mag V-B V magnitude of comparison star B mag JD Julian Date of observation d HII1883, Pleiades H1883 V magnitude of target star, HII 1883 mag H1967 V magnitude of comparison star HII 1967 mag H1954 V magnitude of comparison star HII 1954 mag H1838 V magnitude of comparison star HII 1838 mag JD Julian Date of observation d James Gass ADC 1996 Mar 18 UNKNOWN UNKNOWN March 1996: Original table separated by target star(s) by ADC (James Gass) March 1996: Documentation standardized at ADC (James Gass) J_PASP_105_269.xml CCD photometry of the galactic globular cluster NGC6535 in the B and V passbands J/PASP/106/404 J/PASP/106/404 NGC 6535 BV CCD photometry CCD photometry of the galactic globular cluster NGC6535 in the B and V passbands A Sarajedini Publ. Astron. Soc. Pac. 106 404 1994 1994PASP..106..404S Clusters, globular Photometry, CCD The first CCD color-magnitude diagram (CMD) in B and V is presented for the Galactic globular cluster NGC 6535. From this CMD, which extends below the main-sequence turnoff, we draw the following conclusions: (1) The horizontal branch (HB) is predominantly blue in nature with no RR Lyrae variables known to be cluster members. Nonetheless, based on a comparison with clusters which have blue HBs and RR Lyraes (M15 and M79), we infer a mean HB magnitude of <V(RR)>=15.73+/-0.11 for NGC 6535. (2) Again, via a direct comparison with the blue HBs of M15 and M79, we derive a cluster reddening of E(B-V)=0.44+/-0.02. (3) When combined with the apparent color of the red-giant branch at the level of the HB, (B-V)g=1.18+/-0.02, the derived reddening yields a metal abundance of [Fe/H]=-1.85+/-0.10, similar to that of NGC 6397. (4) Application of the Delta(V(TO-HB)) and Delta((B-V)(SGB-TO)) cluster dating techniques reveals no perceptible age difference between NGC 6535 and NGC 6397. (5) A significant population of nine blue-straggler candidates is detected in NGC 6535. However, this is too few to facilitate a meaningful analysis of their radial distribution.
NGC 6535 C 1801-003 18 03 50.6 -00 17 49
Photometry of NGC 6535 ID Star number --- X X CCD coordinate pix Y Y CCD coordinate pix Vmag Visual magnitude mag B-V B-V color mag o_Vmag Number of observations --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 03-Nov-1994 May 21 Addresses: Sarajedini A. ata@noao.edu Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732, Tucson, Arizona 85726-6732 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 2, 1994 J_PASP_106_404.xml Analyses of Archival Data for Cool Dwarfs. II. A Catalog of Temperatures J/PASP/106/452 J/PASP/106/452 Cool Dwarfs - Temperatures Analyses of Archival Data for Cool Dwarfs. II. A Catalog of Temperatures B J Taylor Publ. Astron. Soc. Pacific 106 452 1994 1994PASP..106..452T Effective temperatures Photometry, Cousins Stars, dwarfs Stars, late-type The file contains values of Cousins R-I and theta [= 5040/T(eff)] for 417 F-K stars which are on or near the main sequence.
The catalog of R-I and theta prefix "vB" for Hyades, "Tr" for Coma stars --- dmsign "+" or "-" for BD stars, blank otherwise --- bd/hd Catalog number (HD if no other labeling) --- bin Binary Components --- wool for number in Woolley et al. 1970 catalog --- hr/w Number in HR or Woolley et al. catalog --- R-I Cousins R-I mag eR-I Standard deviation for Cousins R-I mag theta 5040/T(eff) --- etheta Standard deviation for theta --- B.J. Taylor Brigham Young U. 1994 Aug 04 If there are comments or questions, please contact: Benjamin J. Taylor taylorb@astro.byu.edu Physics and Astronomy Department, ESC Tel.: 801-378-2233 Brigham Young University FAX: 801-378-2265 Provo, UT 84602 J_PASP_106_452.xml vbyHbeta CCD photometry of Melotte 66: a disk analog of Omega Centauri? J/PASP/106/486 J/PASP/106/486 Mel 66 CCD photometry vbyHbeta CCD photometry of Melotte 66: a disk analog of Omega Centauri? B J Anthony-Twarog B A Twarog M Sheeran Publ. Astron. Soc. Pac. 106 486 1994 1994PASP..106..486A Clusters, open Photometry, CCD A CCD study of the peculiar open cluster, Melotte 66, on the vbyHbeta system is presented. The V,(b-y) color-magnitude diagram of this metal-deficient, old disk cluster confirms the anomalous features found in photographic BV studies and extends the main sequence to V=20. The main sequence exhibits a (b-y) color range significantly larger than expected from photometric errors alone; the (b-y) colors are correlated with Hbeta implying that the dispersion is real and is not the result of variable reddening across the cluster. The m1 indices for the turnoff stars imply a spread in [Fe/H] too small to explain the color range. Though the subgiant region is poorly defined, the region above the turnoff in the Hertzsprung gap is richly populated by a group of "yellow stragglers" whose membership is confirmed by radial star counts and radial velocities. The giant branch is richly populated but shows a smaller spread in color at a given V than one would expect from the turnoff region. More important, the giants exhibit a large scatter in m1, in contradiction with the turnoff observations. Various explanations for these observations are discussed, including CN variations among the giants triggered by either binary evolution or rapid rotation among the main-sequence stars.
Photometric indices for Mel 66 stars Haw Hawarden identification number number=1 Hawarden T.G., 1976, MNRAS 243, 492 --- ID Identification number --- X X position pix Y Y position pix Vmag V magnitude (apparent) mag e_Vmag rms uncertainty on V magnitude mag b-y (b-y) color mag e_b-y rms uncertainty on (b-y) color mag m1 m1 index mag e_m1 rms uncertainty on m1 index mag Hbeta Hbeta index --- e_Hbeta rms uncertainty on Hbeta index --- Ny Number of y frames --- Nb Number of b frames --- Nv Number of v frames --- Nw Number of Hbeta wide frames --- Nn Number of Hbeta narrow frames --- Lee Brotzman ADS 1994, Patricia Bauer [CDS] 03-Nov-1994 May 21 Addresses: Anthony-Twarog B.J. anthony@kuphsx.phsx.ukans.edu Twarog B.A. twarog@kuphsx.phsx.ukans.edu Sheeran M. Department of Physics and Astronomy, University of Kansas, Lawrence, Kansas 66045-2151 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 2, 1994 J_PASP_106_486.xml The Spectrum of the Planetary Nebula, IC 418 J/PASP/106/745 J/PASP/106/745 The Spectrum of IC 418 The Spectrum of the Planetary Nebula, IC 418 S Hyung L H Aller W A Feibelman Publ. Astron. Soc. Pac. 106 745 1994 1994PASP..106..745H Planetary nebulae Spectra, ultraviolet A detailed high spectral resolution study of the spectrum of IC 418 is made for the region 3650 A to 10050 A, using the Hamilton echelle spectrograph of Lick Observatory, and of the UV spectral region with archival International Ultraviolet Explorer (IUE) data.
Optical Region line Intensities lam.obs The observed wavelength The observed wavelength in A corrected for the radial velocity, V_{rad} = 37.375 km/s. 0.1nm lam.lab The laboratory wavelength 0.1nm id The line identification --- mult The multiplet number --- k Extinction The extinction coefficient, k_{\lambda}, as tabulated from equations given by Seaton (1979MNRAS.187p..73S) --- I Relative intensity to I(Hbeta=100) the flux I(lam) relative to I(Hbeta) =100 corrected for interstellar extinction, C = log I(H beta)/F(H beta) = 0.21, a value derived by comparing reliable Balmer and Paschen lines. that is, the extinction at lambda 4861 is 0.21 dex. --- F The un-corrected flux relative to F(Hbeta)=100. --- e_F Formal root-mean-square error --- Nancy G. Roman ADC/SDDOO 1995 Mar 20 J_PASP_106_745.xml Secondary Photometric Standard Stars for the Thuan-Gunn and Johnson- Kron-Cousins Systems. J/PASP/106/967 J/PASP/106/967 Secondary Photometric Standard Stars Secondary Photometric Standard Stars for the Thuan-Gunn and Johnson- Kron-Cousins Systems. I Joergensen Publ. Astron. Soc. Pac. 106 967 1994 1994PASP..106..967J Photometry, Cousins Photometry, special systems Photometry, standards CCD photometry is presented for 119 stars observed in the Thuan-Gunn photometric system (the passbands vgr). The sample includes 82 stars for which magnitudes in this system have not previously been published. Photometry in the Johnson-Kron-Cousins photometric system (BV or UBV) has been obtained for a sub-sample of 85 of the stars. Of those stars which are not primary standard stars for the Thuan-Gunn system 70 observed in Gunn r, 48 observed in Gunn g, and 37 observed in Gunn v have sufficient repeat measurements that they may be used as secondary standard stars for CCD photometry. The typical uncertain- ties for the magnitudes of these stars are 0.006 mag.
Standard magnitudes Name Name of star E4, E5, E6, E7, E8, E9: Johnson standard stars from Graham (1982, PASP, 94, 244). N300: Johnson standard stars from Graham (1981, PASP, 93, 29). 1MarkA, PG1633+099, SA92, SA110: Johnson standard stars from Landolt (1992, AJ, 104, 340). F762-9, F1038-6: Stobie et al. (1985, A&AS, 60, 503), not used for the standard calibration. F762-9-2 is variable. BD, Feige, GL745, G18-39, G68-30, HD84937, M67, and Ross: Kent (1985, PASP, 97, 165). Other HD and SA: Zinn (1980, ApJS, 42, 19), not used for the standard calibration. --- V Magnitude in Johnson V mag e_V Mean error on magnitude in Johnson V mag o_V Number of observations in Johnson V --- B-V B-V, Johnson system mag e_B-V Mean error on B-V mag o_B-V Number of observations for B-V --- U-B U-B, Johnson system mag e_U-B Mean error on U-B mag o_U-B Number of observations for U-B --- r Magnitude in Gunn r mag e_r Mean error on magnitude in Gunn r mag o_r Number of observations in Gunn r --- g Magnitude in Gunn g mag e_g Mean error on magnitude in Gunn g mag o_g Number of observations in Gunn g --- v Magnitude in Gunn v mag e_v Mean error on magnitude in Gunn v mag o_v Number of observations in Gunn v --- Nancy G. Roman ADC/SDDOO 1995 Mar 16 This document was prepared by I. Joergensen whom we thank for both the document and the data. It was modified slightly by the undersigned. J_PASP_106_967.xml Infrared Atlas of the Arcturus Spectrum, 0.9-5.3 microns J/PASP/107/1042 J/PASP/107/1042 Infrared Arcturus Atlas Infrared Atlas of the Arcturus Spectrum, 0.9-5.3 microns K Hinkle L Wallace W Livingston Publ. Astron. Soc. Pac. 107 1042 1995 1995PASP..107.1042H Spectra, infrared Spectrophotometry The atlas is contained in 310 spectral files a list of line identifications, plus a file containing a list of the files and unobserved spectral regions. The spectral file names are in the form 'abnnnnn' where 'nnnnn' denotes the spectral region, e.g. file 'ab4300' contains spectra for the 4300-4325 cm-1 range. The atomic and molecular line identifications are in files 'appendix.a' and 'appendix.b', and repeated with a uniform format in file 'lines'. The file 'appendix.c' is a book-keeping device used to correlate the plot plages and spectral files with frequency. See the author-supplied description in 'readme.dat' for more information. A spectral atlas of the infrared spectrum of the bright K2 giant Arcturus has been completed using the 4 meter Mayall telescope and FTS. The 0.9-5.3um spectrum of Arcturus was observed at high signal-to-noise with a resolution of 100,000. Telluric lines were removed by using telluric transmission spectra generated from McMath-Pierce solar spectra or 4 meter lunar spectra. The spectrum of Arcturus was observed on two different dates selected to give large opposite heliocentric shifts. The spectra observed on the different dates have been independently corrected for telluric absorption with the result that the telluric spectrum has been effectively removed from all but the most obscured wavelengths of the Arcturus spectrum. We attempted to identify lines with central depths stronger than a few percent. Identifications seem well in hand with the unidentified lines apparently atomic in origin. The atlas is available either on an AAS CD-ROM or as an ASP monograph.
HR 5340 Arcturus alpha Boo HD 124897 14 15 39.7 +19 10 57
Spectral atlas file 1866- 1875 cm-1 range Spectral atlas file 1873- 1882 cm-1 range Spectral atlas file 1880- 1889 cm-1 range Spectral atlas file 1887- 1896 cm-1 range Spectral atlas file 1894- 1903 cm-1 range Spectral atlas file 1901- 1910 cm-1 range Spectral atlas file 1908- 1917 cm-1 range Spectral atlas file 1915- 1924 cm-1 range Spectral atlas file 1922- 1931 cm-1 range Spectral atlas file 1929- 1938 cm-1 range Spectral atlas file 1936- 1945 cm-1 range Spectral atlas file 1943- 1952 cm-1 range Spectral atlas file 1950- 1959 cm-1 range Spectral atlas file 1957- 1966 cm-1 range Spectral atlas file 1964- 1973 cm-1 range Spectral atlas file 1971- 1980 cm-1 range Spectral atlas file 1978- 1987 cm-1 range Spectral atlas file 1985- 1994 cm-1 range Spectral atlas file 1992- 2001 cm-1 range Spectral atlas file 1999- 2008 cm-1 range Spectral atlas file 2006- 2015 cm-1 range Spectral atlas file 2013- 2022 cm-1 range Spectral atlas file 2020- 2029 cm-1 range Spectral atlas file 2027- 2036 cm-1 range Spectral atlas file 2034- 2043 cm-1 range Spectral atlas file 2041- 2050 cm-1 range Spectral atlas file 2048- 2057 cm-1 range Spectral atlas file 2055- 2064 cm-1 range Spectral atlas file 2062- 2071 cm-1 range Spectral atlas file 2069- 2078 cm-1 range Spectral atlas file 2076- 2085 cm-1 range Spectral atlas file 2083- 2092 cm-1 range Spectral atlas file 2090- 2099 cm-1 range Spectral atlas file 2118- 2127 cm-1 range Spectral atlas file 2125- 2134 cm-1 range Spectral atlas file 2132- 2141 cm-1 range Spectral atlas file 2139- 2148 cm-1 range Spectral atlas file 2146- 2155 cm-1 range Spectral atlas file 2153- 2162 cm-1 range Spectral atlas file 2160- 2169 cm-1 range Spectral atlas file 2167- 2176 cm-1 range Spectral atlas file 2174- 2183 cm-1 range Spectral atlas file 2181- 2190 cm-1 range Spectral atlas file 2398- 2416 cm-1 range Spectral atlas file 2413- 2431 cm-1 range Spectral atlas file 2428- 2446 cm-1 range Spectral atlas file 2443- 2461 cm-1 range Spectral atlas file 2458- 2476 cm-1 range Spectral atlas file 2473- 2491 cm-1 range Spectral atlas file 2488- 2506 cm-1 range Spectral atlas file 2503- 2521 cm-1 range Spectral atlas file 2518- 2536 cm-1 range Spectral atlas file 2533- 2551 cm-1 range Spectral atlas file 2548- 2566 cm-1 range Spectral atlas file 2563- 2581 cm-1 range Spectral atlas file 2578- 2596 cm-1 range Spectral atlas file 2593- 2611 cm-1 range Spectral atlas file 2608- 2626 cm-1 range Spectral atlas file 2623- 2641 cm-1 range Spectral atlas file 2638- 2656 cm-1 range Spectral atlas file 2653- 2671 cm-1 range Spectral atlas file 2668- 2686 cm-1 range Spectral atlas file 2683- 2701 cm-1 range Spectral atlas file 2698- 2716 cm-1 range Spectral atlas file 2713- 2731 cm-1 range Spectral atlas file 2728- 2746 cm-1 range Spectral atlas file 2743- 2761 cm-1 range Spectral atlas file 2758- 2776 cm-1 range Spectral atlas file 2773- 2791 cm-1 range Spectral atlas file 2788- 2806 cm-1 range Spectral atlas file 2803- 2821 cm-1 range Spectral atlas file 2818- 2836 cm-1 range Spectral atlas file 2833- 2851 cm-1 range Spectral atlas file 2848- 2866 cm-1 range Spectral atlas file 2863- 2881 cm-1 range Spectral atlas file 2878- 2896 cm-1 range Spectral atlas file 2893- 2911 cm-1 range Spectral atlas file 2908- 2926 cm-1 range Spectral atlas file 2923- 2941 cm-1 range Spectral atlas file 2938- 2956 cm-1 range Spectral atlas file 2953- 2971 cm-1 range Spectral atlas file 2968- 2986 cm-1 range Spectral atlas file 2983- 3001 cm-1 range Spectral atlas file 2998- 3016 cm-1 range Spectral atlas file 3013- 3031 cm-1 range Spectral atlas file 3028- 3046 cm-1 range Spectral atlas file 3043- 3061 cm-1 range Spectral atlas file 3058- 3076 cm-1 range Spectral atlas file 3073- 3091 cm-1 range Spectral atlas file 3088- 3106 cm-1 range Spectral atlas file 3103- 3121 cm-1 range Spectral atlas file 3118- 3136 cm-1 range Spectral atlas file 3133- 3156 cm-1 range Spectral atlas file 3148- 3171 cm-1 range Spectral atlas file 3163- 3186 cm-1 range Spectral atlas file 3178- 3201 cm-1 range Spectral atlas file 3193- 3216 cm-1 range Spectral atlas file 3208- 3231 cm-1 range Spectral atlas file 3223- 3246 cm-1 range Spectral atlas file 3238- 3261 cm-1 range Spectral atlas file 3253- 3276 cm-1 range Spectral atlas file 3268- 3291 cm-1 range Spectral atlas file 3283- 3306 cm-1 range Spectral atlas file 3298- 3321 cm-1 range Spectral atlas file 3313- 3336 cm-1 range Spectral atlas file 3328- 3351 cm-1 range Spectral atlas file 3343- 3366 cm-1 range Spectral atlas file 3358- 3381 cm-1 range Spectral atlas file 3373- 3396 cm-1 range Spectral atlas file 3388- 3411 cm-1 range Spectral atlas file 3403- 3426 cm-1 range Spectral atlas file 3418- 3441 cm-1 range Spectral atlas file 3433- 3456 cm-1 range Spectral atlas file 3448- 3471 cm-1 range Spectral atlas file 3997- 4027 cm-1 range Spectral atlas file 4022- 4052 cm-1 range Spectral atlas file 4047- 4077 cm-1 range Spectral atlas file 4072- 4102 cm-1 range Spectral atlas file 4097- 4127 cm-1 range Spectral atlas file 4122- 4152 cm-1 range Spectral atlas file 4147- 4177 cm-1 range Spectral atlas file 4172- 4202 cm-1 range Spectral atlas file 4197- 4227 cm-1 range Spectral atlas file 4222- 4252 cm-1 range Spectral atlas file 4247- 4277 cm-1 range Spectral atlas file 4272- 4302 cm-1 range Spectral atlas file 4297- 4327 cm-1 range Spectral atlas file 4322- 4352 cm-1 range Spectral atlas file 4347- 4377 cm-1 range Spectral atlas file 4372- 4402 cm-1 range Spectral atlas file 4397- 4427 cm-1 range Spectral atlas file 4422- 4452 cm-1 range Spectral atlas file 4447- 4477 cm-1 range Spectral atlas file 4472- 4502 cm-1 range Spectral atlas file 4497- 4527 cm-1 range Spectral atlas file 4522- 4552 cm-1 range Spectral atlas file 4547- 4577 cm-1 range Spectral atlas file 4572- 4602 cm-1 range Spectral atlas file 4597- 4627 cm-1 range Spectral atlas file 4622- 4652 cm-1 range Spectral atlas file 4647- 4677 cm-1 range Spectral atlas file 4672- 4702 cm-1 range Spectral atlas file 4697- 4727 cm-1 range Spectral atlas file 4722- 4752 cm-1 range Spectral atlas file 4747- 4777 cm-1 range Spectral atlas file 4772- 4802 cm-1 range Spectral atlas file 4797- 4827 cm-1 range Spectral atlas file 4822- 4852 cm-1 range Spectral atlas file 4847- 4877 cm-1 range Spectral atlas file 4872- 4902 cm-1 range Spectral atlas file 4897- 4927 cm-1 range Spectral atlas file 4922- 4952 cm-1 range Spectral atlas file 4947- 4977 cm-1 range Spectral atlas file 4972- 5002 cm-1 range Spectral atlas file 4997- 5027 cm-1 range Spectral atlas file 5022- 5052 cm-1 range Spectral atlas file 5047- 5077 cm-1 range Spectral atlas file 5072- 5102 cm-1 range Spectral atlas file 5097- 5127 cm-1 range Spectral atlas file 5122- 5152 cm-1 range Spectral atlas file 5147- 5177 cm-1 range Spectral atlas file 5472- 5502 cm-1 range Spectral atlas file 5497- 5527 cm-1 range Spectral atlas file 5522- 5552 cm-1 range Spectral atlas file 5547- 5577 cm-1 range Spectral atlas file 5572- 5602 cm-1 range Spectral atlas file 5597- 5627 cm-1 range Spectral atlas file 5622- 5652 cm-1 range Spectral atlas file 5647- 5677 cm-1 range Spectral atlas file 5672- 5702 cm-1 range Spectral atlas file 5697- 5727 cm-1 range Spectral atlas file 5722- 5752 cm-1 range Spectral atlas file 5747- 5777 cm-1 range Spectral atlas file 5772- 5802 cm-1 range Spectral atlas file 5797- 5827 cm-1 range Spectral atlas file 5822- 5852 cm-1 range Spectral atlas file 5847- 5877 cm-1 range Spectral atlas file 5872- 5902 cm-1 range Spectral atlas file 5897- 5927 cm-1 range Spectral atlas file 5922- 5952 cm-1 range Spectral atlas file 5947- 5977 cm-1 range Spectral atlas file 5972- 6002 cm-1 range Spectral atlas file 5997- 6027 cm-1 range Spectral atlas file 6022- 6052 cm-1 range Spectral atlas file 6047- 6077 cm-1 range Spectral atlas file 6072- 6102 cm-1 range Spectral atlas file 6097- 6127 cm-1 range Spectral atlas file 6122- 6152 cm-1 range Spectral atlas file 6147- 6177 cm-1 range Spectral atlas file 6172- 6202 cm-1 range Spectral atlas file 6197- 6227 cm-1 range Spectral atlas file 6222- 6252 cm-1 range Spectral atlas file 6247- 6277 cm-1 range Spectral atlas file 6272- 6302 cm-1 range Spectral atlas file 6297- 6327 cm-1 range Spectral atlas file 6322- 6352 cm-1 range Spectral atlas file 6347- 6377 cm-1 range Spectral atlas file 6372- 6402 cm-1 range Spectral atlas file 6397- 6427 cm-1 range Spectral atlas file 6422- 6452 cm-1 range Spectral atlas file 6447- 6477 cm-1 range Spectral atlas file 6472- 6502 cm-1 range Spectral atlas file 6497- 6527 cm-1 range Spectral atlas file 6522- 6552 cm-1 range Spectral atlas file 6547- 6577 cm-1 range Spectral atlas file 6572- 6602 cm-1 range Spectral atlas file 6597- 6627 cm-1 range Spectral atlas file 6622- 6652 cm-1 range Spectral atlas file 6647- 6677 cm-1 range Spectral atlas file 7397- 7427 cm-1 range Spectral atlas file 7422- 7452 cm-1 range Spectral atlas file 7447- 7477 cm-1 range Spectral atlas file 7472- 7502 cm-1 range Spectral atlas file 7497- 7527 cm-1 range Spectral atlas file 7522- 7552 cm-1 range Spectral atlas file 7547- 7577 cm-1 range Spectral atlas file 7572- 7602 cm-1 range Spectral atlas file 7597- 7627 cm-1 range Spectral atlas file 7622- 7652 cm-1 range Spectral atlas file 7647- 7677 cm-1 range Spectral atlas file 7672- 7702 cm-1 range Spectral atlas file 7697- 7727 cm-1 range Spectral atlas file 7722- 7752 cm-1 range Spectral atlas file 7747- 7777 cm-1 range Spectral atlas file 7772- 7802 cm-1 range Spectral atlas file 7797- 7827 cm-1 range Spectral atlas file 7822- 7852 cm-1 range Spectral atlas file 7847- 7877 cm-1 range Spectral atlas file 7872- 7902 cm-1 range Spectral atlas file 7897- 7927 cm-1 range Spectral atlas file 7922- 7952 cm-1 range Spectral atlas file 7947- 7977 cm-1 range Spectral atlas file 7972- 8002 cm-1 range Spectral atlas file 7997- 8027 cm-1 range Spectral atlas file 8022- 8052 cm-1 range Spectral atlas file 8047- 8077 cm-1 range Spectral atlas file 8072- 8102 cm-1 range Spectral atlas file 8097- 8127 cm-1 range Spectral atlas file 8122- 8152 cm-1 range Spectral atlas file 8147- 8177 cm-1 range Spectral atlas file 8172- 8202 cm-1 range Spectral atlas file 8197- 8227 cm-1 range Spectral atlas file 8222- 8252 cm-1 range Spectral atlas file 8247- 8277 cm-1 range Spectral atlas file 8272- 8302 cm-1 range Spectral atlas file 8297- 8327 cm-1 range Spectral atlas file 8322- 8352 cm-1 range Spectral atlas file 8347- 8377 cm-1 range Spectral atlas file 8372- 8402 cm-1 range Spectral atlas file 8397- 8427 cm-1 range Spectral atlas file 8422- 8452 cm-1 range Spectral atlas file 8447- 8477 cm-1 range Spectral atlas file 8472- 8502 cm-1 range Spectral atlas file 8497- 8527 cm-1 range Spectral atlas file 8522- 8552 cm-1 range Spectral atlas file 8547- 8577 cm-1 range Spectral atlas file 8572- 8602 cm-1 range Spectral atlas file 8597- 8627 cm-1 range Spectral atlas file 8622- 8652 cm-1 range Spectral atlas file 8647- 8677 cm-1 range Spectral atlas file 8672- 8702 cm-1 range Spectral atlas file 8697- 8727 cm-1 range Spectral atlas file 8722- 8752 cm-1 range Spectral atlas file 8747- 8777 cm-1 range Spectral atlas file 8772- 8802 cm-1 range Spectral atlas file 8797- 8827 cm-1 range Spectral atlas file 8822- 8852 cm-1 range Spectral atlas file 8847- 8877 cm-1 range Spectral atlas file 8872- 8902 cm-1 range Spectral atlas file 8896- 8953 cm-1 range Spectral atlas file 8946- 9003 cm-1 range Spectral atlas file 8996- 9053 cm-1 range Spectral atlas file 9046- 9103 cm-1 range Spectral atlas file 9096- 9153 cm-1 range Spectral atlas file 9146- 9203 cm-1 range Spectral atlas file 9196- 9253 cm-1 range Spectral atlas file 9246- 9303 cm-1 range Spectral atlas file 9296- 9353 cm-1 range Spectral atlas file 9346- 9403 cm-1 range Spectral atlas file 9396- 9453 cm-1 range Spectral atlas file 9446- 9503 cm-1 range Spectral atlas file 9496- 9553 cm-1 range Spectral atlas file 9546- 9603 cm-1 range Spectral atlas file 9596- 9653 cm-1 range Spectral atlas file 9646- 9703 cm-1 range Spectral atlas file 9696- 9753 cm-1 range Spectral atlas file 9746- 9803 cm-1 range Spectral atlas file 9796- 9853 cm-1 range Spectral atlas file 9846- 9903 cm-1 range Spectral atlas file 9896- 9953 cm-1 range Spectral atlas file 9946-10003 cm-1 range Spectral atlas file 9996-10053 cm-1 range Spectral atlas file 10046-10103 cm-1 range Spectral atlas file 10096-10153 cm-1 range Spectral atlas file 10146-10203 cm-1 range Spectral atlas file 10196-10253 cm-1 range Spectral atlas file 10246-10303 cm-1 range Spectral atlas file 10296-10353 cm-1 range Spectral atlas file 10346-10403 cm-1 range Spectral atlas file 10396-10453 cm-1 range Spectral atlas file 10446-10503 cm-1 range Spectral atlas file 10496-10553 cm-1 range Spectral atlas file 10546-10603 cm-1 range Spectral atlas file 10596-10653 cm-1 range Spectral atlas file 10646-10703 cm-1 range Spectral atlas file 10696-10753 cm-1 range Spectral atlas file 10746-10803 cm-1 range Spectral atlas file 10796-10853 cm-1 range Spectral atlas file 10846-10903 cm-1 range Spectral atlas file 10896-10953 cm-1 range Freq Frequency scale in wavenumbers cm-1 ObsS Observed Arcturus spectrum in summer --- TelS Telluric spectrum in summer --- RatS Ratioed spectrum in summer --- ObsW Observed Arcturus spectrum in winter --- TelW Telluric spectrum in winter --- RatW Ratioed spectrum in winter --- List of Atomic and Molecular identified lines Freq Frequency in wavenumbers cm-1 Name Ion or Molecule name --- Note Notes concerning the line --- CDS 1996 Jan 26 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 5, 1995 Lee Brotzman [ADS] 07-Nov-1995 J_PASP_107_1042.xml Catalog of Photoelectric Measures of Occultation Binary Stars J/PASP/107/299 J/PASP/107/299 Occultation Binaries Catalog Catalog of Photoelectric Measures of Occultation Binary Stars B D Mason Publ. Astron. Soc. Pac. 107 299 1995 1995PASP..107..299M Occultations Stars, double and multiple occultations binaries: visual catalogs The observation of lunar occultation phenomena allows for the determination of binary star data which can not always be obtained using classical techniques. No complete catalog has been compiled since that of Evans (1981a) in spite of a 99% increase in the available data. This catalog presents a catalog of photoelectric and occultation measures of binary and multiple systems complete through 1994.
occultation objects and measures Name Common Name --- AddName Additional Name --- HD/HDE HD or HDE Designation (if available) --- SAO SAO Designation (if available) --- RAh Right Ascension hours (2000.0) h RAdm Right ascension minutes (2000.0) 0.1min DE- Sign of declination (2000.0) --- DEd Declination degrees (2000.0) deg DEm Declination minutes (2000.0) arcmin EpochB of Observation in Besselian years yr EpochH of Observation in HJD-2400000 d P.A. Position angle of direction vector deg Sep. Vector separation in mas mas e_Sep. Sigma in separation mas Del-m Delta-m in magnitudes mag e_Del-m Sigma in delta-m mag Lambda Central wavelength of filter nm delta-L FWHM of filter nm Note Note detailed in file "notes.dat" --- Ref1 First Reference (see file "refs.dat") --- Ref2 Second reference (see file "refs.dat") --- Notes to occulcat.dat Note Note designation, as in file "occulcat.dat" --- Text Text of Note (eventually on several lines) --- All references RefCode Reference code, as in file "occult.dat" --- Text Text of reference (eventually on several lines) --- occulcat.doc Explanation of catalog Brian Mason Georgia State U 1995 Jul 06 UNKNOWN UNKNOWN * 20-May-1998: notes.dat and refs.dat were transformed into data tables (from original files occulcat.not and occulcat.ref) at CDS (F. Ochsenbein) UNKNOWN UNKNOWN Additonal information on the construction of the catalog is provided in occulcat.doc. The notes to the catalog are in occulcat.not and the references in occulcat.ref. J_PASP_107_299.xml Secondary Photometric Standards for Northern Nova-Like Cataclysmic Variables J/PASP/107/324 J/PASP/107/324 Northern CV secondary photometric standards Secondary Photometric Standards for Northern Nova-Like Cataclysmic Variables A A Henden R K Honeycutt Publ. Astron. Soc. Pac. 107 324 1995 1995PASP..107..324H V/94 : Catalog and Atlas of Cataclysmic Variables (Downes+ 1997) Binaries, cataclysmic Novae Photometry An average of 11 B, V secondary standards per field have been established for 58 cataclysmic variable stars, most of which are nova-like variables. The standards are within a few arcminutes of the variable and are therefore well-suited for CCD photometry. The standards have brightness of V~12-17 and have a typical accuracy per standard of +0.02mag.
Program star fields Name Star name --- OtheName Other name --- Type Variability type number=1 From CV catalog of Downes and Shara, 1993, See Cat. <V/94> am : AM Herculis variable cv : cataclysmic variable dq : DQ Herculis variable n : nova nl : novalike variable non-cv: not a cataclysmic variable ug : U Gem variable ux : novalike variable (UX UMa subtype) vy : novalike variable (VY Scl subtype) pec : peculiar : : uncertain :: : very uncertain --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Magnitudes and Colors Star Star name --- DRA Offset in right ascension number=1 Offset from the cataclysmic variable (position in table2), positive north and east arcsec DDE Offset in declination number=1 Offset from the cataclysmic variable (position in table2), positive north and east arcsec n_Vmag Number of observations --- Vmag V magnitude mag e_Vmag rms uncertainty on Vmag mag B-V B-V colour index mag e_B-V rms uncertainty on B-V mag James Marcout, Patricia Bauer CDS 1997 Jul 24 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_PASP_107_324.xml A catalog of the youngest YSOs and candidate protostars. J/PASP/107/617 J/PASP/107/617 YSOs and candidate protostars catalog. A catalog of the youngest YSOs and candidate protostars. M D Pollanen P A Feldman Publ. Astron. Soc. Pac. 107 617 1995 1995PASP..107..617P Stars, peculiar YSOs We have compiled a catalog of candidate protostars from the major astronomical journals up to the end of 1993. The Belchman-Ichikawa color criterion was used as the main test of an author's claim that a source should be deemed a candidate protostar. Names, positions (1950 and 2000), LSR velocities, information on whether there are associated outflows, and references are provided. This catalog is meant to update an earlier compilation by Wynn-Williams (1982). Copyright: 1995, Astronomical Society of the Pacific, reproduced with permission.
Catalogue of the youngest YSOs and candidate protostars Name Source name, alternate name in parentheses number=1 Object name as given in the reference. Alternate names are listed in parentheses. An asterisk in the name field indicates the name was taken from the IRAS catalogue. --- IRAS IRAS name number=2 Designation from the IRAS Point Source Catalogue with a few exceptions. IRAS source names are listed when they are given explicitly in the reference and/or are widely known and used. --- RAh Right ascension 1950 h RAm Right ascension 1950 min RAs Right ascension 1950 s DE- Declination sign 1950 --- DEd Declination 1950 deg DEm Declination 1950 arcmin DEs Declination 1950 arcsec n_DEs Note on DE number=3 An asterisk indicates that the coordinate was taken from the IRAS catalogue. --- RAh2000 Right ascension 2000 h RAm2000 Right ascension 2000 min RAs2000 Right ascension 2000 s DE-2000 Declination sign 2000 --- DEd2000 Declination 2000 deg DEm2000 Declination 2000 arcmin DEs2000 Declination 2000 arcsec V(LSR) Local-standard-of-rest velocity km/s dash when a second V(LSR) exists --- V2(LSR) Second Local-standard-of-rest velocity km/s Outflow Information about outflow number=4 Y an outflow was observed to be associated with the source N an outflow was not found P an outflow was observed but it remains unclear whether the outflow is associated with the source - No information on outflow is available --- Ref Reference code number=5 Reference codes to the paper(s) from which the information was extracted. The reference for each line applies to all the information on that line with the exception of the items marked with an asterisk (*), which were obtained directly from the IRAS catalogue. See References below. --- Francois Ochsenbein CDS 1995 Nov 13 Marco Pollanen <pollan@gh1.hia.nrc.ca> J_PASP_107_617.xml Stars classified as constant in the General Catalogue of Variable Stars. II. J/PASP/108/1105 J/PASP/108/1105 Constant Stars in the GCVS. II. Stars classified as constant in the General Catalogue of Variable Stars. II. E G Schmidt Publ. Astron. Soc. Pac. 108 1105 1996 1996PASP..108.1105S II/139 : General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988) Photometry Stars, variable Photometric observations have been made of 36 stars classified as CST or CST: in the General Catalogue of Variable Stars. Six of these stars are found to vary and three others were deemed possible variables. Of the certain variables, two (MR Her and TY Sge) are red pulsators, one (V1585 Cyg) is a rapid irregular variable, one is apparently a short period Cepheid-strip star (V432 Oph), one is an eclipsing binary (AQ Boo) and one is uncertain type (V351 Cyg). The stars we have observed as MR Her and TY Sge are the same ones which were identified on finding charts in the discovery papers suggesting that these stars have intervals of variability and intervals of quiescence. V432 Oph is of special interest because our photometry indicates that it may be either a double mode Cepheid or a peculiar long period RR Lyrae star depending on which of a couple of possible periods turns out to be correct.
Photometric data for 51 variable stars Name Star name --- HJD Heliocentric Julian Date d Vmag V magnitude mag Rmag R magnitude mag V-R V-R color mag Flag Flag indicating uncertainty --- Patricia Bauer CDS 1997 Feb 11 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 09-Nov-1996 J_PASP_108_1105.xml On the determination of empirical stellar flux scales J/PASP/108/313 J/PASP/108/313 Empirical stellar flux scales On the determination of empirical stellar flux scales J C Hall Publ. Astron. Soc. Pac. 108 313 1996 1996PASP..108..313H Spectrophotometry Several studies have appeared in the literature describing methods for deriving stellar continuum fluxes as simple functions of Johnson color indices. In previous papers, we have used similar relations to derive Ca II H & K line core fluxes for dwarf stars on Lowell Observatory's Solar-Stellar Spectrograph (SSS) program. Our desire is to present our data, and complementary data from the Mt. Wilson and National Solar Observatory stellar and solar programs, in terms of physical fluxes. However, our existing relations break down for mid-K and later stars and for giant stars, which form an important element of our target list. In this work I have used a broader range of spectrophotometry and angular diameters than in our previous work to derive empirical flux scales for spectral types A to early M, luminosity classes I to V, and for four color indices, Johnson B-V, V-R, R-I, and Stromgren b-y. In this paper I describe the methods I used and present the derived flux scales. I compare the results with those from earlier studies and present examples of the use of the flux scales. The data and results are available on the World Wide Web home page. Access <http://www.lowell.edu>, select "Lowell staff", and select the author's home page.
Empirical flux scales Bandpass Bandpass The continuum flux of a star of color index X in one of the three bandpasses given in the table is: F(cont)=(C0+(C1*X))+/-[sigmad(dex), or ~sigmap(%)], with units of mW/m2/(0.1nm). Any pair of coefficients [C0, C1] applies only to the indicated luminosity classes, and only to the indicated color range. Due to rapidly decreasing numbers of data points at the extrema of the color range (resulting from the difficulty of doing spectrophotometry at those extrema, particularly for K and M stars), the fits degrade rapidly beyond the indicated ranges. --- CI Color index --- C0 Zeroth-order coefficient of flux scale These are the coefficients to be entered in a relation of the form log(F(lambda))=C0+C1(CI), C0 is the zeroth-order coefficient, C1 is the first-order coefficient, and CI is the color index corresponding to those coefficients. --- C1 First-order coefficient of flux scale --- sigmad Error in dex of flux scale relation --- sigmap Error in percent of flux scale relation % CRb Blue end of CI range These fields indicate the range of the particular color index for which a pair of flux-scale coefficients may be used. A flux-scale relation should never be applied outside these limits, because of the many quantities that go into deriving the stellar continuum fluxes, as well as the rapidly changing and uncertain nature of these quantities at the color index extrema (e.g.blanketing). mag CRr Red end of CI range mag LC Luminosity classes --- Table of references HD Henry Draper Catalogue number --- Name Star name --- rSp Spectrophotometric references rSp is the spectrophotometric references for the star. The main reference used in making the flux scales is listed first. Other references are listed in parentheses, "()". Standard stars of Taylor (1984ApJS...54..167T) and Hayes & Latham (1975, ApJ 197, 593) are listed in angle brackets, "<>". Abbreviations for all references are as follows: B76 = Breger (1976ApJS...32....7B) BEM78 = Barnes, Evans, & Moffett (1978MNRAS.183..285B) BL94 = Blackwell & Lynas-Gray (1994A&A...282..899B) BHNT66 = Baschek et al. (1966ZA.....65..418B) BO65 = Baschek & Oke (1965ApJ...141.1404B) CB70 = Crawford & Barnes (1970AJ.....75..946C) DP71 = Dickens & Penny (1971MNRAS.153..287D) HL75 = Hayes & Latham (1975ApJ...197L..55H) HM90 = Hauck & Mermilliod (1990A&AS...86..107H) J66 = Jones 1966; (in Spectral Classification and Multicolor Photometry, IAU Symp. 24, p.141) KTK88 = Kharitonov et al. 1988; (The Spectroscopic Catalog of Stars, Alma-Ata, Nauka) O67 = Oke (1967ApJ...150..513O) OC66 = Oke & Conti (1966ApJ...143..134O) O74 = Oinas (1974ApJS...27..405O) R69 = Rodriguez (1969, ApJ 5, 125) S65 = Stromgren & Perry 1965 (Photoelectric uvby photometry for 1217 stars brighter than V=6.5, mostly of spectral class A, F, & G (Princeton, Institute for Advanced Study)) S71 = Stickland (1971MNRAS.153..501S) SPO71 = Schild, Peterson, & Oke (1971ApJ...166...95S) T84 = Taylor (1984ApJS...54..259T) vP76 = van Paradijs (1976A&AS...24...53V) W65 = Willstrop (1965, MmRAS 69, 83) W67 = Whiteoak (1967ApJ...150..521W) WBSB62 = Wildey et al. (1962ApJ...135...94W) --- rD Reference for star's angular diameter --- rBl Reference for blanketing coefficients --- rb-y Reference for Stromgren b-y index --- Stellar properties HD Star's Henry Draper Catalogue number --- Sp Spectral type and luminosity class --- D Star's angular diameter mas e_D Error in D mas Vmag V magnitude mag B-V Johnson B-V color mag V-R Johnson V-R color mag R-I Johnson R-I color mag b-y Stromgren b-y color mag Line blanketing coefficients Lambda Central wavelength of bandpass The central wavelength of a 50-A wide bandpass to which the coefficients in the same row are applicable. 0.1nm C0 Zeroth-order polynomial coefficient --- C1 First-order polynomial coefficient --- C2 Second-order polynomial coefficient --- C3 Third-order polynomial coefficient --- C4 Fourth-order polynomial coefficient --- sigma Std. dev. of data points about the fit --- CRb Bluest color index for the fit mag CRr Reddest color index for the fit mag LC0 Luminosity class for C0 (no = blank) --- LC1 Luminosity class for C1 (no = blank) --- LC2 Luminosity class for C2 (no = blank) --- LC3 Luminosity class for C3 (no = blank) --- LC4 Luminosity class for C4 (no = blank) --- CI Color index for coefficient --- CDS 1996 Sep 06 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 6, 1996 Lee Brotzman [ADS] 07-May-1996 J_PASP_108_313.xml Low-Mass Stars in Outer Field in NGC 6397 J/PASP/108/682 J/PASP/108/682 Low-Mass Stars in Outer Field in NGC 6397 Low-Mass Stars in Outer Field in NGC 6397 J R Mould A M Watson J S Gallagher III G E Ballester C J Burrows S Casertano J T Clarke D Crisp R E Griffiths J Hester J G Hoessel J A Holtzman P A Scowen K R Stapelfeldt J T Trauger J A Westphal Pub. Astron. Soc. Pacific 108 682 1996 1996PASP..108..682M Colors Galaxies, photometry Photometry, infrared Stars, Population II I magnitudes and V-I colors are given for 700 stars in a region 10' north of the center of the cluster NGC 6397. X and Y coordinates are also provided. The observations were made with the Hubble Space Telescope to study the luminosity distribution in a population II sample.
The catalog ID Running number of star on chip --- V-I V-I color mag I I magnitude mag chip Chip number --- X Pixel number in X pix Y Pixel number in Y pix N. G. Roman ADC/SSDOO 1996 Dec 23 J_PASP_108_682.xml Secondary Photometric Standards for Northern Cataclysmic Variables and Related Objects J/PASP/109/441 J/PASP/109/441 Northern Cataclysmic Variables Secondary Photometric Standards for Northern Cataclysmic Variables and Related Objects A A Henden R K Honeycutt Publ. Astron. Soc. Pac. 109 441 1997 1997PASP..109..441H Binaries, cataclysmic Photometry, CCD An average of 30 B,V secondary standards per field have been established for 76 variable stars. These are mostly cataclysmic variables of various subclasses but also include a variety of other kinds of variable stars. The standards are within a few arc minutes of the variable and are therefore well suited for CCD photometry. The standards have brightnesses of V~12-17 and have a typical accuracy per standard of +/-0.01mag. (c) Astronomical Society of the Pacific
Magnitudes and colors Star Name of CV star --- --- Always '-' --- Std Number of the standard star --- dRA Offset in R.A. from CV (N through E) arcsec dDE Offset in Dec. from CV (N through E) arcsec Nobs Number of observations --- Vmag V magnitude mag e_Vmag Error in Vmag mag B-V B-V color mag e_B-V Error in B-V mag table3.tex AASTeX version of table3.dat CDS 1997 Jul 04 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 07-May-1997 J_PASP_109_441.xml Light Curves For 40 Field RR Lyrae Variables J/PASP/109/524 J/PASP/109/524 Light Curves for 40 RR Lyraes Light Curves For 40 Field RR Lyrae Variables A C Layden Publ. Astron. Soc. Pac. 109 524 1997 1997PASP..109..524L Photometry, CCD Stars, variable Photoelectric photometry in the BV passbands is presented for 33 nearby RR Lyrae stars. CCD frames are used to recalibrate the photographic photometry of an additional 7 RR Lyraes to the Johnson B band. Light curves are presented for all 40 stars, along with derived light curve parameters. For one subset of stars, reddenings and distances are computed from the observed colors at minimum light, periods, mean magnitudes, and spectroscopic metal abundances taken from the literature. For a second subset of stars, metal abundances, distances, and reddenings are determined via Fourier decomposition of the light curves. The results of the two methods are compared. (c) Astronomical Society of the Pacific
Photoelectric photometry data Star Variable star name --- HJD Heliocentric Julian Date JD Phase Photometric phase --- Vmag V magnitude mag e_Vmag Error in Vmag mag B-V B-V color mag e_B-V Error in B-V mag CDS 1997 Jul 04 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 8, 1997 Lee Brotzman [ADS] 07-May-1997 J_PASP_109_524.xml Rotational Velocities of Intermediate-mass Main Sequence Stars J/PASP/109/759 J/PASP/109/759 Rotational Velocities of Intermediate-mass MS Stars Rotational Velocities of Intermediate-mass Main Sequence Stars S C Wolff T Simon Publ. Astron. Soc. Pac. 109 759 1997 1997PASP..109..759W Rotational velocities Spectroscopy Stars, normal Rotational velocities are reported for intermediate-mass main-sequence stars selected from Gray (1986, Gray and Garrison 1987, 1989a, 1989b). Measured rotational velocities, with photometric data from SIMBAD, are given in table1.dat for 249 stars. The measurements are based on new, high-S/N CCD spectra from the Coude Feed Telescope of the Kitt Peak National Observatory. Published velocities for 294 stars are provided in table2.dat. (from Publ. Astron. Soc. Pac. 109, 759 (1997)) We analyze these rotation rates for a dependence on both mass and age. We compare the average rotation speeds of the field stars with mean velocities for young stars in Orion, the {Alpha} Persei cluster, the Pleiades, and the Hyades. The average rotation speeds of stars more massive than ~1.6 Msol experience little or no change during the evolutionary lifetimes of these stars on the zero age main sequence (ZAMS) or within the ZAMS band. Less massive stars in the range between 1.6 Msol and 1.3 Msol also show little decline in mean rotation rate while they are on the main sequence, and at most a factor of two decrease in velocity as they evolve off the main sequence. The e-folding time for the loss of angular momentum by the latter group of stars is at least 1-2 billion years. This inferred characteristic time scale for spindown is far longer than the established rotational braking time for solar-type stars with masses below ~1.3 Msol. We conclude from a comparison of the trends in rotation with trends in chromospheric and coronal activity that the overall decline in mean rotation speed along the main sequence, from ~2 Msol down to ~1.3 Msol, is imposed during the pre-main-sequence phase of evolution, and that this pattern changes little thereafter while the star resides on the main sequence. The magnetic activity must therefore play only a minor role in determining the rotation rates of the intermediate-mass stars, either because a solar-like dynamo is weak or absent, or else the geometry of the magnetic field is appreciably less effective in removing angular momentum from these stars.
Measured rotational velocities HD HD number --- B-V B-V color index Photometric data from SIMBAD. --- beta H{beta} index --- b-y b-y color index --- c1 c1 index --- mag Absolute magnitude MV mag l_vsini Limit flag on V*Sin(i) --- vsini Measured V*Sin(i) km/s bin Bin in Fig. 3(a), color-magnitude A blank indicates that the star lies beyond the terminal age main sequence (TAMS). --- Published rotational velocities HD HD number --- B-V B-V color index --- beta H{beta} index --- b-y b-y color index --- c1 c1 index --- mag Absolute magnitude MV mag l_vsini Limit flag on V*Sin(i) --- vsini Published V*Sin(i) km/s bin Bin in Fig. 3(a), color-magnitude A blank indicates that the star lies beyond the terminal age main sequence (TAMS). --- ref Reference code 1 = Slettebak et al. 1975 2 = Kraft 1967b 3 = Danziger and Faber 1972 4 = Soderblom 1983 5 = Benz and Mayor 1984 --- Julie Anne Watko SSDOO/ADC 1998 Jan 08 The ADC thanks Dr. Simon for providing the data tables as LaTeX files. J.A. Watko [SSDOO/ADC] converted the tables to ASCII. J_PASP_109_759.xml Probing the LHS Catalog I. New Nearby Stars and the Coolest Subdwarf J/PASP/109/849 J/PASP/109/849 Probing the LHS Catalog Probing the LHS Catalog I. New Nearby Stars and the Coolest Subdwarf J E Gizis I N Reid Publ. Astron. Soc. Pac. 109 849 1997 1997PASP..109..849G V/70 : CNS3 (Nearby Stars, Preliminary 3rd Version; Gliese+ 1991) III/198 : PMSU (Palomar/MSU nearby star spectroscopic survey; Hawley+ 1997) Space velocities Spectroscopy Stars, distances Stars, M-type Stars, nearby Stars, subdwarf We present moderate resolution spectroscopy of 111 cool dwarf stars to supplement the observations we have already presented in the Palomar/MSU Nearby-Star Spectroscopic Survey. The sample consists of 71 suspected nearby stars added to the Preliminary Third Catalog of Nearby Stars since 1991 as well as 40 faint red stars selected from the LHS catalog. The study was aimed at identifying interesting red dwarfs, particularly new nearby, ultracool dwarfs, and very metal-poor stars. The observations were made using the Palomar 60-inch, the Hale 200-inch and the Las Campanas 100-inch telescopes between June 1995 and January 1996. The spectral resolution is approximately 3 Angstroms per pixel with wavelength coverage from 6200 to 7500 Angstroms. Table 2 contains bandstrengths for TiO, CaH, and CaOH indices.
Candidate nearby stars: basic data (table 1) Name Star name Gl - Gliese (1969, Veroff. Astr. Rechen-Instituts, Heidelberg, Nr. 22) GJ - Gliese & Jahreiss =1979A&AS...38..423G Wo - Woolley et al (1970, R. Obs. Ann., No. 5) =Cat. <V/32> LHS - Luyten Half-Second Catalogue =Cat. <I/87> LTT - Luyten Two-Tenths Catalogue LP - Luyten Palomar proper-motion catalogue G - Giclas et al (1971, Lowell Proper Motion Survey) =Cat. <I/79> Steph - Stephenson (1986, AJ, 91, 137) =Cat. <III/123> (Nomenclature note: should be named "StKM") --- Bin Primary or secondary binary comp. Components in a binary system are identified as p (primary) or s (secondary, tertiary). --- Note1 Individual Note b G 035-027 and LP 469-118: Photometry based upon Fleming et al. (1988) observed V_{system} = 14.20 and assumed Delta V = 0.42 c Steph 2.908: This is the 809th star in Stephenson (1986). Photometry is from Weis (1991). d BD+28 3698: Jahreiss notes that this object is presumably a dK binary with Delta m = 0.8, see Heintz (1993). The distance was estimated by Jahreiss. e LHS 3705: This is also Cou 2234. Estimated distance assumes the system is a binary with Delta m = 0.0 as determined by Couteau (1985). --- RAh Right ascension, 2000 h RAm Right ascension, 2000 min RAs Right ascension, 2000 s DE- Declination sign --- DEd Declination, 2000 deg DEm Declination, 2000 arcmin DEs Declination, 2000 arcsec Src Source of positional data Source of positional data: 5- Digital Sky Survey Codes 1-4 were used in Reid et al. (1995),Hawley et al. (1996), Hawley+ (1997) --- MV Absolute V magnitude mag r Distance Distance and estimated uncertainty (%) from the authors' data, using a weighted combination of trigonometric and spectroscopic parallaxes. pc er Distance uncertainty % wPi Weight for trigonometric parallax An entry of -1 indicates that Jahreiss's distance estimates were adopted. % wSp Weight for spectroscopic parallax % SpType Spectral type --- Vmag Apparent V magnitude mag Candidate nearby stars: bandstrengths (table 2) Name Star name --- TiO1 TiO1 index: F(6718-6723)/F(6703-6708) --- TiO2 TiO2 index: F(7058-7061)/F(7043-7046) --- TiO3 TiO3 index: F(7092-7097)/F(7079-7084) --- TiO4 TiO4 index: F(7130-7135)/F(7115-7120) --- TiO5 TiO5 index: F(7126-7135)/F(7042-7046) --- CaH1 CaH1 index: F(6380-6390)/F (6345-6355,6410-6420)) --- CaH2 CaH2 index: F(6814-6846)/F(7042-7046) --- CaH3 CaH3 index: F(6960-6990)/F(7042-7046) --- CaOH CaOH index: F(6230-6240)/F(6345-6354) --- Halpha H-alpha Eq. Width 0.1nm Candidate nearby stars: Space Velocities Name Star name --- pmRA Proper motion in right ascension, from CNS3 arcsec/yr pmDE Proper motion in declination, from CNS3 arcsec/yr RV Radial velocity km/s U U space velocity km/s V V space velocity km/s W W space velocity km/s MV Absolute V magnitude (from table1.dat) mag Faint LHS stars Name Star name LHS - Luyten Half-Second Catalogue =Cat. <I/87> --- Note1 Individual Note a Probably misidentified. --- mr r magnitude from Luyten (1979) --- TiO5 TiO5 index: F(7126-7135)/F(7042-7046) --- CaH1 CaH1 index: F(6380-6390)/F (6345-6355,6410-6420)) --- CaH2 CaH2 index: F(6814-6846)/F(7042-7046) --- CaH3 CaH3 index: F(6960-6990)/F(7042-7046) --- Halpha H alpha Equivalent Width 0.1nm SpType Spectral Type --- RV Radial Velocity km/s John Gizis U.Mass 1997 Nov 14 J_PASP_109_849.xml Galactic globular cluster metallicity scale from the Ca II triplet I. Catalog J/PASP/109/883 J/PASP/109/883 Globular metallicity scale. I. Galactic globular cluster metallicity scale from the Ca II triplet I. Catalog G A Rutledge J E Hesser P B Stetson M Mateo L Simard M Bolte E D Friel Y Copin Publ. Astron. Soc. Pac. 109 883 1997 1997PASP..109..883R VII/195 : Globular Clusters in the Milky Way (Harris, 1996) Rutledge et al., Paper II. 1997PASP..109..907R Clusters, globular Photometry, calcium triplet Radial velocities We have obtained 2640 CCD spectra with resolution ~4{AA} in the region 7250-9000{AA} for 976 stars lying near the red giant branches in color-magnitude diagrams of 52 Galactic globular clusters. Radial velocities of ~16km/s accuracy per star determined from the spectra are combined with other criteria to assess quantitative membership probabilities. Measurements of the equivalent widths of the infrared calcium triplet lines yield a relative metal-abundance ranking with a precision that compares favorably to other techniques. Regressions between our system and those of others are derived. Our reduction procedures are discussed in detail, and the resultant catalog of derived velocities and equivalent widths is presented. The metal abundances derived from these data will be the subject of a future paper. (c) Astronomical Society of the Pacific
Individual star data and results Cluster Cluster name Name of the globular cluster, repeated for each observed star in that cluster. The authors also included the following alternative names for some clusters: NGC 104 = 47 Tuc NGC 6273 = M 19 NGC 4590 = M 68 NGC 6637 = M 69 NGC 5904 = M 5 NGC 6681 = M 70 NGC 6093 = M 80 NGC 6717 = Pal 9 NGC 6121 = M 4 NGC 6809 = M 55 NGC 6171 = M 107 NGC 6981 = M 72 NGC 6218 = M 12 NGC 7089 = M 2 NGC 6254 = M 10 NGC 7099 = M 30 NGC 6266 = M 62 --- Star Star name --- DRV Calulated velocity minus cluster velocity Difference between the authors' calculated velocity of the star (see Section 4 of the printed paper) and the velocity given in the MWGC catalog (Cat. <VII/195>. km/s V(HB)-Vmag V magnitude of star above the horizontal branch mag (B-V)0 Dereddened B-V color Dereddened B-V color of the star determined with E(B-V) from the MWGC catalog. mag dCa Weighted mean {SIGMA}Ca (net Ca II index) of the star 0.1nm e_dCa External error of dCa 0.1nm Pmu Probability of membership from proper-motion data % Pvel Probability of membership from our calculated velocities % fp f_p_ value The f_p, f_r, and final weight, w, respectively, used in the authors' fitting technique to calculate the reduced equivalent width, W' of the the cluster. See Section 6 of the printed paper for technique, and Table 2 of the paper for W' values; the weight has been scaled in each cluster --- fr f_r_ value --- w w value --- Nspect Number of spectra analyzed for the star --- Night Night the star was observed The nights the star was observed, where the first number indicates the observing run, and the other numbers indicate the specific night of observation. Therefore, 1-1 represents 1989 April 13, 1-2 represents 1989 April 14, ..., and 2-1 represents 1989 July 13. --- Notes Notes 0: Star not used to compute reduced EW for cluster, 1: See cluster notes in Appendix A, 2: Weak TiO present, 3: Strong TiO present, 4: Possible AGB star, 5: Possible HB star, 6: Non-cluster member based on position in CMD, 7: Crowded field, 8: Uncertain ID, 9: Star has weak {SIGMA}Ca for V_HB - V position, 10: Star has strong {SIGMA}Ca for V_HB - V position, 11: Suntzeff & Kraft (1996AJ....111.1913S) suggest that line strength is variable. --- table9.tex AASTeX version of table9.dat table9.ps PostScript version CDS 1998 Feb 06 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 04-Nov-1997 J_PASP_109_883.xml CG Muscae: a cataclysmic misclassification J/PASP/109/977 J/PASP/109/977 VI photometry of CG Muscae CG Muscae: a cataclysmic misclassification A C Layden S Wachter Publ. Astron. Soc. Pac. 109 977 1997 1997PASP..109..977L Photometry Stars, variable We have obtained extensive photometry of the suspected cataclysmic variable CG Muscae, and find that it is in fact an RR Lyrae star. We measure its light curve parameters and derive physical parameters including metal abundance, reddening, and distance. We also have discovered three new variables in the nearby field. We suspect that two are contact binary stars, while the third is too faint to determine its variability type with certainty. (c)Astronomical Society of the Pacific
CG Mus 12 20 13.7 -74 13 16 V2 12 19 56.7 -74 10 51 V3 12 19 39.4 -74 06 31 V4 12 20 58.7 -74 08 34
Photometric data Star Star name --- HJD Heliocentric Julian Date of observation JD Vmag V magnitude mag e_Vmag Error in Vmag mag Imag I magnitude mag e_Imag Error in Imag mag Phase Photometric phase --- CDS 1998 Feb 06 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 04-Nov-1997 J_PASP_109_977.xml Stromgrem uvby photometry of the magnetic chemically peculiar stars HR 1643, Theta Aur, 49 Cam, and HR 3724 J/PASP/109/9 J/PASP/109/9 Photometry of chemically peculiar stars Stromgrem uvby photometry of the magnetic chemically peculiar stars HR 1643, Theta Aur, 49 Cam, and HR 3724 S J Adelman Publ. Astron. Soc. Pac. 109 9 1997 1997PASP..109....9A J/A+AS/103/1 : 63 And, HD 192913, HR 8240 & 108 Aqr (Adelman+ 1994) J/A+AS/106/333 : Alpha And, HD 184905, HR 8216 & HR 8434 (Adelman+ 1994) J/A+AS/114/253 : HD 11187, HD 14940, HD 15144, 20 Eri, HR 8933 (Adelman+ 1995) Photometry, uvby Stars, peculiar Differential Stromgren uvby photometric observations from the Four College Automated Photoelectric Telescope of four magnetic Chemically Peculiar stars are used to refine rotational periods and to define the shapes of the light curves. HR 1643 (P=2.73475d) shows large phase variability in all four magnitudes. Theta Aur (P=3.6188d) exhibits large amplitude variations with two components contributing to the minima. For 49 Cam (P=4.28679d), we probably are observing both polar regions and much of the surface. The values for HR 3724 (P=33.984d) confirm Wolff's result that the main variability is in v.
HR 1643 HD 32650 BN Cam 05 12 22.4 +73 56 49 theta Aur HD 40312 HR 2095 37 Aur 05 59 43.0 +37 12 49 HD 62140 49 Cam HR 2977 BC Cam 07 46 27.6 +62 49 53 HR 3724 HD 81009 KU Hya 09 22 50.9 -09 50 19
uvby Photometry for HR 1643 uvby Photometry for Theta Aur uvby Photometry for 49 Cam uvby Photometry for HR 3724 HJD Heliocentric Julian Date d u(v-c) variable-comparison (v-c) u magnitude mag u(ch-c) check-comparison (ch-c) u magnitude mag b(v-c) variable-comparison (v-c) b magnitude mag b(ch-c) check-comparison (ch-c) b magnitude mag v(v-c) variable-comparison (v-c) v magnitude mag v(ch-c) check-comparison (ch-c) v magnitude mag y(v-c) variable-comparison (v-c) y magnitude mag y(ch-c) check-comparison (ch-c) y magnitude mag Averaged values Star Star name --- Per Period considered number=1 Period considered: For HR 1643: year 2: from 2448531.9511 to 2448605.8525 year 3: from 2449019.7156 to 2449058.6251 year 4: from 2449253.8931 to 2449411.6532 year 5: from 2449644.9089 to 2449754.7141 For 49 Cam : year 1: from 2448207.8560 to 2448332.6985 year 3: from 2449086.6603 to 2449088.6600 year 4: from 2449344.9103 to 2449445.6397 year 5: from 2449688.9632 to 2449815.6664 For HR 3724 : year 1: from 2448212.9338 to 2448354.7019 year 2: from 2448568.0029 to 2448750.6338 year 3: from 2449009.7602 to 2449111.6652 year 4: from 2449334.9479 to 2449482.6388 year 5: from 2449676.9983 to 2449839.6395 --- u(v-c) variable-comparison (v-c) u magnitude mag e_u(v-c) rms uncertainty on (v-c) u magnitude mag u(ch-c) check-comparison (ch-c) u magnitude mag e_u(ch-c) rms uncertainty on (ch-c) u magnitude mag b(v-c) variable-comparison (v-c) b magnitude mag e_b(v-c) rms uncertainty on (v-c) b magnitude mag b(ch-c) check-comparison (ch-c) b magnitude mag e_b(ch-c) rms uncertainty on (ch-c) b magnitude mag v(v-c) variable-comparison (v-c) v magnitude mag e_v(v-c) rms uncertainty on (v-c) v magnitude mag v(ch-c) check-comparison (ch-c) v magnitude mag e_v(ch-c) rms uncertainty on (ch-c) v magnitude mag y(v-c) variable-comparison (v-c) y magnitude mag e_y(v-c) rms uncertainty on (v-c) y magnitude mag y(ch-c) check-comparison (ch-c) y magnitude mag e_y(ch-c) rms uncertainty on (ch-c) y magnitude mag Patricia Bauer CDS 1997 Feb 11 UNKNOWN UNKNOWN AAS CD-ROM series, Volume 7, 1996 Lee Brotzman [ADS] 04-Nov-1996 J_PASP_109_9.xml The supernova rate in starburst galaxies J/PASP/110/553 J/PASP/110/553 Supernova rate in starburst galaxies The supernova rate in starburst galaxies M W Richmond A V Filippenko J Galisky Publ. Astron. Soc. Pac. 110 553 1998 1998PASP..110..553R Magnitudes, absolute Redshifts Supernovae We conducted an optical CCD search for supernovae in a sample of 142 bright [m(B)<=16mag], nearby (z<=0.03) starburst galaxies over the period 1988 December to 1991 June, to a limiting R-band magnitude of 18. Five supernovae were found, in all cases outside the host galaxy's nucleus. We determine supernova rates (in supernova units or SNU) in the extranuclear regions to be 0.7h^2^SNU for Type Ia, 0.7h^2^SNU for Type Ib/c, and 0.6h^2^SNU for Type II, with large uncertainties but upper limits of 2.2h^2^, 2.5h^2^, and 1.7h^2^SNU, respectively. These rates are similar to those measured in "normal" galaxies. We found no evidence for a supernova-induced brightening in any galactic nucleus and, with a few reasonable assumptions, can place upper limits of 9h^2^, 12h^2^, and 7h^2^SNU on the rates of unobscured supernovae Types Ia, Ib/c, and II, respectively, inside the nuclei.
Supernova rate in starburst galaxies Name Galaxy name --- Bmag B magnitude mag n_Bmag Note on Bmag number=3 d: Value taken from Soifer et al. (1987ApJ...320..238S) and corrected as follow: m=m_b_(Soifer)-0.09. --- z Redshift --- AV V absorption mag M0B Absolute B magnitude number=1 Calculated using H_0_=57km/s/Mpc, and corrected for Galactic extinction mag M0Rnuc Nuclear absolute R magnitude number=2 Within a circular aperture of diameter 5.8" centered on nucleus mag log(FIR) log_10_ of far-IR flux [solLum] James Marcout, Patricia Bauer CDS 1998 Jun 22 UNKNOWN UNKNOWN From the electronic version of PASP J_PASP_110_553.xml Accurate Positions for MCG Galaxies J/PASP/110/779 J/PASP/110/779 Accurate Positions for MCG Galaxies Accurate Positions for MCG Galaxies H G Corwin Jr. I Pesenson M Schmitz D -C Kim J Bennett B F Madore J M Mazzarella G Helou Publ. Astron. Soc. Pac. 110 779 1998 1998PASP..110..779C Galaxy catalogs Positional data We have measured accurate celestial coordinates for over 4000 extragalactic objects primarily drawn from a list of MCG galaxies with no recently published accurate positions. We used IPAC's Skyview program to display FITS images clipped from the Digitized Sky Survey, and to measure the coordinates. The standard deviations in the new positions depend slightly on the measurement command used, but are on the order of 1.0 arcsec to 1.2 arcsec (internal errors). The table of data includes all the duplicate measurements we made, as well as corrections and additions made after the PASP paper was submitted, so has 5120 entries.
Accurate positions Name NED name --- RAh Right Ascension hours (J2000.0) h RAm Right Ascension minutes (J2000.0) min RAs Right Ascension seconds (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination degrees (J2000.0) deg DEm Declination minutes of arc (J2000.0) arcmin DEs Declination seconds of arc (J2000.0) arcsec Method Method of measurement The method of measurement is "P" for measurements using Skyview's "pick" command, or "E" for measurements using the "examine" command. --- Survey Sky survey name The digitized sky survey plate is "E" for the POSS1 103a-E red plates, and "J" for the SERC IIIa-J blue-green plates. --- Harold G. Corwin, Jr. NED/IPAC/Caltech 1998 Jul 09 Skyview was produced at IPAC under NASA contract NAS7-918. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under US Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope at Siding Spring. The NASA/IPAC Extragalactic Database (NED) is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Areonautics and Space Administration. J_PASP_110_779.xml A Stellar Spectral Flux Library: 1150 - 25000 A J/PASP/110/863 J/PASP/110/863 A Stellar Spectral Flux Library: 1150 - 25000 A A Stellar Spectral Flux Library: 1150 - 25000 A A J Pickles Publ. Astron. Soc. Pac. 110 863 1998 1998PASP..110..863P Atlases Spectrophotometry Available published spectra have been combined to form a library of digital stellar spectra spanning 1150 - 25000 A with a sampling interval of 5 A and a resolution of ~500. The library was constructed to enable synthesis and modeling of the integrated light from composite populations. The library consists of 131 flux-calibrated spectra, encompassing all normal spectral types and luminosity classes at solar abundance, plus metal-weak and metal-rich F-K dwarfs and G-K giants. Each library spectrum was formed by combining data from several sources overlapping in wavelength coverage. The data sources are listed in file srclist.doc, and the specific components used to form each spectrum are identified in file complist.doc. The library has complete spectral coverage from 1150 - 10620 A for all spectra and to 25000 A for about half of them, mainly later types of solar abundance. Missing spectral coverage in the infrared consists of a smooth energy distribution formed from standard colors for the relevant types. The library spectra are each given as normalized F-lambda vs. wavelength in A: each spectrum is normalized to 1.0 at 5556 A. Spectra are organized in two groups of 131 files each; the files are named according to the spectral type, luminosity class and metallicity. The first group of files, designated UVILIB, contains the final combined spectra from 1150 - 11620 A. The second set of files, UVKLIB, extends the UVILIB spectra out to 25000 A, as described above. The data files contain the wavelength, normalized flux and standard deviation for the final combined spectrum in the first three columns. Subsequent columns contain the normalized flux for component spectra which were used to make the final spectrum. Columns which contain these component spectra are labelled according to a code which specifies the source of that spectrum (see complist.doc for more detail) -- UVILIB component codes Code Occasional Alternate Reference source Codes Fsv Sviderskiene 1988 fi (IUE) Heck et al. 1984 fg Gunn & Stryker 1983 fk Kiehling 1987 fj Jacoby, Hunter & Christian 1984 fs Silva & Cornell 1992 fp Pickles 1985 fn (N6522) Pickles & van der Kruit 1990 fr fr1, fr2 Serote Roos, Boisson & Joly 1996 fd fdd1, fdd2; fd3, fd4 Danks & Dennefeld 1994 UVKLIB component codes Code Reference source Fh spectrum from UVILIB fse interpolated spectrum based on standardized flux points fl Lancon & Rocca-Volmerange 1992 fd Dallier, Boisson & Joly 1996 fk Kleinmann & Hall 1986 fc Cohen et al. (1995, 1996a, 1996b) fm Fluks et al. 1994 M giant spectra in UVKLIB include the synthetic M0-M10 MK type spectra from Fluks et. al. (1994), and are a combination of these and the UVILIB spectra in the range 1150-10620A. M0-M8 III are the only cases where the 1150-10500A data differ between UVILIB and UVKLIB. M9 and M10 III spectra are exclusively synthetic spectra from Fluks et. al. (1994) in both libraries. In addition to the spectrum library itself, synthetic photometry and selected local equivalent widths & magnitude indices are provided in tables synphot.dat and lew.dat. The standard infrared colors used to form the smooth energy curves used in UVKLIB spectra are listed in irstphot.dat. Further documentation details are available in the *.doc files as described below in the table notes in this ReadMe.
physical data & synthetic photometry num spectrum number (range 1-131) --- nsv info on spectra used from Sviderskiene 1988 Meanings of the following values of nsv: 1 - indicates a spectrum used to check the spectral energy distribution, but not included in the component combination 2 - indicates the average of two spectra used similarly 3 - indicates a spectrum that was actually used in the combination, generally in the uv 4 - indicates the average of two spectra used similarly --- ni no. of spectra used from Heck+ 1984 --- ng no. of spectra used from Gunn & Stryker 1983 --- nk no. of spectra used from Kiehling 1987 --- nj no. of spectra used from Jacoby+ 1984 --- ns no. of spectra used from Silva+ 1992 --- np no. of spectra used from Pickles 1985 --- nn no. of spectra used from Pickles+ 1990 --- nr no. of spectra used from Serote Roos+ 1996 --- ndd no. of spectra used from Danks+ 1994 --- nl no. of spectra used from Lancon+ 1992 --- nd no. of spectra used from Dallier+ 1996 --- nkh no. of spectra used from Kleinmann+ 1986 --- nc no. of spectra used from Cohen+ 1995,1996 --- SpType spectral type Prefix 'r' refers to metal-rich abundance. Prefix 'w' refers to metal-weak abundance. --- LogTe log of effective temperature --- U3-V U3-V color mag B3-V B3-V color mag V-Rc V-Rc color mag V-Ic V-Ic color mag V-J V-J color mag V-H V-H color mag V-K V-K color mag [Fe/H] metallicity index [Fe/H] Estimated from the Mg b/MgH and Fe blend features. [Sun] Mbol bolometric magnitude Calculation of Mbol for M giants used extension of spectrum out to 100,000 A (Fluks 1994 synthetic M III spectra). mag BCv bolometric correction, V band M(V) = Mbol - BCv; set so that BCv(G5V)=4.75-4.83=-0.08 M(Ic) = Mbol - BCi M(K) = Mbol - BCk mag BCi bolometric correction, Ic band mag BCk bolometric correction, K band mag FlamV avg. f-lambda/f(5556 A) within V bandpass FlamV is the average F(lambda) for each spectrum within the V filter passband, and is used to compensate for the fact that the library spectra are normalized at 5556A, rather than the effective wavelength (ElamV) of the V filter, which varies for each spectrum. --- ElamV effective lambda of V filter, this spectrum 0.1nm uRMS rms in ultraviolet region --- oRMS rms in optical region --- lRMS rms in 14300 - 25000 A region --- iRMS rms in (near) infrared region --- local equiv. widths of selected features num spectrum number (range 1-131) --- SpType spectral type Prefix 'r' refers to metal-rich abundance. Prefix 'w' refers to metal-weak abundance. --- G43 local equiv. width for G band 0.1nm MgH local equiv. width for MgH/Mg b band 0.1nm Mg2 magnitude index for Mg band Mg2 = -2.5 log (F_line/F_continuum). mag Fe4380 local equiv. width for Fe I blend, 4380 A 0.1nm Fe5270 local equiv. width for Fe I blend, 5270 A 0.1nm Fe5385 local equiv. width for Fe I blend, 5385 A 0.1nm Hdelta local equiv. width for Balmer H-delta 0.1nm Hgamma local equiv. width for Balmer H-gamma 0.1nm Hbeta local equiv. width for Balmer H-beta 0.1nm Halpha local equiv. width for Balmer H-alpha 0.1nm CaHK local equiv. width for Ca II H&K 0.1nm CaT local equiv. width for Ca triplet (~8500 A) The local equivalent width LEW is defined as LEW=(lam2-lam1)*(1-2.*(F_line/(F_bluecontinuum + F_redcontinuum))). where lam1 and lam2 are the minimum and maximum wavelengths defining the line region. The wavelength ranges defining the line, red continuum and blue continuum regions for each feature are given in the file linecont.doc. 0.1nm uvCN local equiv. width for uv CN band (~3840 A) 0.1nm irCN local equiv. width for ir CN band (~9230 A) 0.1nm D4000 amplitude of the 4000 A flux break Defined as the ratio of the average flux (per unit frequency, f_nu) in the wavelength range 4050-4250 A to that in the range 3750-3950 A (e.g., Hamilton, D., 1985, ApJ 297, 371). Actually calculated here by summing F(lambda)*lambda^2 over the (4050-4250 A) and (3750 - 3950 A) regions and then taking the ratio, i.e., D_4000 = \Sigma_{4050}^{4250} F_\nu \Delta\nu / \Sigma_{3750}^{3950} F_\nu \Delta\nu = \Sigma_{4050}^{4250} F_\lambda \lambda^2 / \Sigma_{3750}^{3950} F_\lambda \lambda^2 mag [Fe/H] metallicity index [Fe/H] [Sun] standard ir photometry for each spectrum num spectrum number (range 1-131) --- SpType spectral type Prefix 'r' refers to metal-rich abundance. Prefix 'w' refers to metal-weak abundance. --- V-J V-J color mag V-H V-H color mag V-K V-K color mag V-L V-L color mag O5 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- O9 V (1150-10620 A) B5-7 V (1150-10620 A) A2 V (1150-10620 A) B1-2 III (1150-10620 A) B3 III (1150-10620 A) B5 III (1150-10620 A) B9 III (1150-10620 A) A0 III (1150-10620 A) B0 I (1150-10620 A) B5 I (1150-10620 A) B8 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- B0 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fs f(lambda)/f(5556 A) for component fs --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- B1 V (1150-10620 A) A5 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- B3 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- B8 V (1150-10620 A) A0 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fd f(lambda)/f(5556 A) for component fd --- B9 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- fd f(lambda)/f(5556 A) for component fd --- A0 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- fs f(lambda)/f(5556 A) for component fs --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- A3 V (1150-10620 A) metal-weak F5 V (1150-10620 A) metal-rich F6 V (1150-10620 A) F8 V (1150-10620 A) metal-weak G0 V (1150-10620 A) metal-rich G0 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- A7 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fdd1 f(lambda)/f(5556 A) for component fdd1 --- fdd2 f(lambda)/f(5556 A) for component fdd2 --- F0 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fr f(lambda)/f(5556 A) for component fr --- F2 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fp f(lambda)/f(5556 A) for component fp --- fdd1 f(lambda)/f(5556 A) for component fdd1 --- fdd2 f(lambda)/f(5556 A) for component fdd2 --- F5 V (1150-10620 A) metal-weak F8 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fp f(lambda)/f(5556 A) for component fp --- fs f(lambda)/f(5556 A) for component fs --- F6 V (1150-10620 A) G2 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fk f(lambda)/f(5556 A) for component fk --- fd1 f(lambda)/f(5556 A) for component fd1 --- fd2 f(lambda)/f(5556 A) for component fd2 --- metal-rich F8 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fk f(lambda)/f(5556 A) for component fk --- G0 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fp f(lambda)/f(5556 A) for component fp --- fd f(lambda)/f(5556 A) for component fd --- G5 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fp f(lambda)/f(5556 A) for component fp --- fd1 f(lambda)/f(5556 A) for component fd1 --- metal-weak G5 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- metal-rich G5 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fk f(lambda)/f(5556 A) for component fk --- G8 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fk f(lambda)/f(5556 A) for component fk --- K0 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- fd1 f(lambda)/f(5556 A) for component fd1 --- fd2 f(lambda)/f(5556 A) for component fd2 --- metal-rich K0 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fk f(lambda)/f(5556 A) for component fk --- fg f(lambda)/f(5556 A) for component fg --- fs f(lambda)/f(5556 A) for component fs --- fr1 f(lambda)/f(5556 A) for component fr1 --- fr2 f(lambda)/f(5556 A) for component fr2 --- K2 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- fd1 f(lambda)/f(5556 A) for component --- K3 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fs f(lambda)/f(5556 A) for component fs --- fr f(lambda)/f(5556 A) for component fr --- K4 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fp f(lambda)/f(5556 A) for component fp --- fk f(lambda)/f(5556 A) for component fk --- K5 V (1150-10620 A) M6 V (1150-10620 A) K1 IV (1150-10620 A) K3 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- K7 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- M1 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fp f(lambda)/f(5556 A) for component fp --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- M2 V (1150-10620 A) K2 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- M2.5 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fp f(lambda)/f(5556 A) for component fp --- fd f(lambda)/f(5556 A) for component fd --- M3 V (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fs f(lambda)/f(5556 A) for component fs --- fj f(lambda)/f(5556 A) for component fj --- M4 V (1150-10620 A) M5 V (1150-10620 A) metal-weak K1 III (1150-10620 A) metal-weak K4 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- B2 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fd f(lambda)/f(5556 A) for component fd --- fr f(lambda)/f(5556 A) for component fr --- B6 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- A4-7 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fs f(lambda)/f(5556 A) for component fs --- F0-2 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd3 f(lambda)/f(5556 A) for component fd3 --- fd4 f(lambda)/f(5556 A) for component fd4 --- F5 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fk f(lambda)/f(5556 A) for component fk --- fdd1 f(lambda)/f(5556 A) for component fdd1 --- fdd2 f(lambda)/f(5556 A) for component fdd2 --- F8 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fs f(lambda)/f(5556 A) for component fs --- fk f(lambda)/f(5556 A) for component fk --- fd f(lambda)/f(5556 A) for component fd --- G0 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fr f(lambda)/f(5556 A) for component fr --- G2 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- G5 IV (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fp f(lambda)/f(5556 A) for component fp --- fk f(lambda)/f(5556 A) for component fk --- fr f(lambda)/f(5556 A) for component fr --- G8 IV (1150-10620 A) K0 III (1150-10620 A) K3 III (1150-10620 A) K5 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- fd f(lambda)/f(5556 A) for component fd --- M0 V (1150-10620 A) K0 IV (1150-10620 A) K1 III (1150-10620 A) M2 III (1150-10620 A) M7 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fd f(lambda)/f(5556 A) for component fd --- O8 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- A3 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- A5 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- A7 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- F0 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fk f(lambda)/f(5556 A) for component fk --- fp f(lambda)/f(5556 A) for component fp --- fd f(lambda)/f(5556 A) for component fd --- F2 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- F5 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fk f(lambda)/f(5556 A) for component fk --- fp f(lambda)/f(5556 A) for component fp --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- G0 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fk f(lambda)/f(5556 A) for component fk --- G5 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fj f(lambda)/f(5556 A) for component fj --- fp f(lambda)/f(5556 A) for component fp --- fr f(lambda)/f(5556 A) for component fr --- fk f(lambda)/f(5556 A) for component fk --- fd f(lambda)/f(5556 A) for component fd --- metal-weak G5 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- metal-rich G5 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- fn f(lambda)/f(5556 A) for component fn --- G8 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- metal-weak G8 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- fn f(lambda)/f(5556 A) for component fn --- metal-weak K0 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fd f(lambda)/f(5556 A) for component fd --- fn f(lambda)/f(5556 A) for component fn --- metal-rich K0 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- metal-rich K1 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fk f(lambda)/f(5556 A) for component fk --- fp f(lambda)/f(5556 A) for component fp --- fr f(lambda)/f(5556 A) for component fr --- fn f(lambda)/f(5556 A) for component fn --- metal-weak K2 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fn f(lambda)/f(5556 A) for component fn --- fd f(lambda)/f(5556 A) for component fd --- metal-rich K2 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- metal-weak K3 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fp f(lambda)/f(5556 A) for component fp --- fn f(lambda)/f(5556 A) for component fn --- metal-rich K3 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fk f(lambda)/f(5556 A) for component fk --- fr f(lambda)/f(5556 A) for component fr --- fn f(lambda)/f(5556 A) for component fn --- K4 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fp f(lambda)/f(5556 A) for component fp --- metal-rich K4 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fj f(lambda)/f(5556 A) for component fj --- fk f(lambda)/f(5556 A) for component fk --- fp f(lambda)/f(5556 A) for component fp --- fs f(lambda)/f(5556 A) for component fs --- fn f(lambda)/f(5556 A) for component fn --- metal-rich K5 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fs f(lambda)/f(5556 A) for component fs --- fp f(lambda)/f(5556 A) for component fp --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- fn f(lambda)/f(5556 A) for component fn --- M0 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- M1 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fk f(lambda)/f(5556 A) for component fk --- fp f(lambda)/f(5556 A) for component fp --- fs f(lambda)/f(5556 A) for component fs --- fr f(lambda)/f(5556 A) for component fr --- M3 III (1150-10620 A) M5 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- M4 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fr f(lambda)/f(5556 A) for component fr --- M6 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fp f(lambda)/f(5556 A) for component fp --- fd f(lambda)/f(5556 A) for component fd --- M8 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fg f(lambda)/f(5556 A) for component fg --- fd f(lambda)/f(5556 A) for component fd --- M9 III (1150-10620 A) M10 III (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- B2 II (1150-10620 A) A0 I (1150-10620 A) A2 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fsv f(lambda)/f(5556 A) for component fsv --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- B5 II (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fsv f(lambda)/f(5556 A) for component fsv --- fd f(lambda)/f(5556 A) for component fd --- F0 II (1150-10620 A) F2 II (1150-10620 A) G5 II (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- K0-1 II (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fk f(lambda)/f(5556 A) for component fk --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- K3-4 II (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fk f(lambda)/f(5556 A) for component fk --- fd f(lambda)/f(5556 A) for component fd --- M3 II (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fsv f(lambda)/f(5556 A) for component fsv --- fk f(lambda)/f(5556 A) for component fk --- B1 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fs f(lambda)/f(5556 A) for component fs --- fj f(lambda)/f(5556 A) for component fj --- fsv f(lambda)/f(5556 A) for component fsv --- B3 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fs f(lambda)/f(5556 A) for component fs --- fj f(lambda)/f(5556 A) for component fj --- fsv f(lambda)/f(5556 A) for component fsv --- fd f(lambda)/f(5556 A) for component fd --- F0 I (1150-10620 A) F8 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- F5 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- G0 I (1150-10620 A) M2 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- G2 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fr f(lambda)/f(5556 A) for component fr --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- G5 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- G8 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fi f(lambda)/f(5556 A) for component fi --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fsv f(lambda)/f(5556 A) for component fsv --- K2 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- fsv f(lambda)/f(5556 A) for component fsv --- K3 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fk f(lambda)/f(5556 A) for component fk --- fj f(lambda)/f(5556 A) for component fj --- fs f(lambda)/f(5556 A) for component fs --- fd f(lambda)/f(5556 A) for component fd --- fr f(lambda)/f(5556 A) for component fr --- K4 I (1150-10620 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fk f(lambda)/f(5556 A) for component fk --- fd f(lambda)/f(5556 A) for component fd --- fr f(lambda)/f(5556 A) for component fr --- fsv f(lambda)/f(5556 A) for component fsv --- O5 V (1150-25000 A) A2 V (1150-25000 A) A3 V (1150-25000 A) G5 V (1150-25000 A) F2 V (1150-25000 A) F5 V (1150-25000 A) F5 IV (1150-25000 A) G8 IV (1150-25000 A) A7 III (1150-25000 A) K1 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fl f(lambda)/f(5556 A) for component fl --- O9 V (1150-25000 A) B0 V (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fd f(lambda)/f(5556 A) for component fd --- fl f(lambda)/f(5556 A) for component fl --- B1 V (1150-25000 A) B5-7 V (1150-25000 A) B8 V (1150-25000 A) B9 V (1150-25000 A) A5 V (1150-25000 A) A7 V (1150-25000 A) F0 V (1150-25000 A) metal-weak F5 V (1150-25000 A) metal-rich F6 V (1150-25000 A) metal-weak F8 V (1150-25000 A) metal-rich F8 V (1150-25000 A) B5 II (1150-25000 A) F0 II (1150-25000 A) F2 II (1150-25000 A) G5 II (1150-25000 A) K0-1 II (1150-25000 A) B0 I (1150-25000 A) B3 I (1150-25000 A) B5 I (1150-25000 A) A0 I (1150-25000 A) A2 I (1150-25000 A) F8 I (1150-25000 A) metal-weak G0 V (1150-25000 A) metal-rich G0 V (1150-25000 A) metal-weak G5 V (1150-25000 A) metal-rich G5 V (1150-25000 A) K4 V (1150-25000 A) K5 V (1150-25000 A) M0 V (1150-25000 A) M1 V (1150-25000 A) M3 V (1150-25000 A) M4 V (1150-25000 A) M6 V (1150-25000 A) B6 IV (1150-25000 A) A0 IV (1150-25000 A) A4-7 IV (1150-25000 A) F0-2 IV (1150-25000 A) G0 IV (1150-25000 A) G5 IV (1150-25000 A) K0 IV (1150-25000 A) K1 IV (1150-25000 A) K3 IV (1150-25000 A) O8 III (1150-25000 A) B3 III (1150-25000 A) B5 III (1150-25000 A) B9 III (1150-25000 A) A0 III (1150-25000 A) A3 III (1150-25000 A) A5 III (1150-25000 A) F0 III (1150-25000 A) F2 III (1150-25000 A) F5 III (1150-25000 A) B2 II (1150-25000 A) metal-rich K5 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- B2 IV (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fd f(lambda)/f(5556 A) for component fd --- B3 V (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fd f(lambda)/f(5556 A) for component fd --- fl f(lambda)/f(5556 A) for component fl --- A0 V (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fl f(lambda)/f(5556 A) for component fl --- fc f(lambda)/f(5556 A) for component fc --- F6 V (1150-25000 A) M2 V (1150-25000 A) M5 V (1150-25000 A) F8 IV (1150-25000 A) G8 I (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fl f(lambda)/f(5556 A) for component fl --- fk f(lambda)/f(5556 A) for component fk --- G8 V (1150-25000 A) K3 V (1150-25000 A) F8 V (1150-25000 A) G0 V (1150-25000 A) K7 V (1150-25000 A) K4 III (1150-25000 A) G2 I (1150-25000 A) B1 I (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fl f(lambda)/f(5556 A) for component fl --- fd f(lambda)/f(5556 A) for component fd --- G2 V (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fc f(lambda)/f(5556 A) for component fc --- fl f(lambda)/f(5556 A) for component fl --- fk f(lambda)/f(5556 A) for component fk --- K0 V (1150-25000 A) K2 V (1150-25000 A) M2.5 V (1150-25000 A) G2 IV (1150-25000 A) B1-2 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fd f(lambda)/f(5556 A) for component fd --- metal-rich K0 V (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fl f(lambda)/f(5556 A) for component fl --- fd f(lambda)/f(5556 A) for component fd --- fk f(lambda)/f(5556 A) for component fk --- G0 III (1150-25000 A) G8 III (1150-25000 A) K0 III (1150-25000 A) G5 III (1150-25000 A) K4 I (1150-25000 A) M2 I (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fl f(lambda)/f(5556 A) for component fl --- fd f(lambda)/f(5556 A) for component fd --- fk f(lambda)/f(5556 A) for component fk --- K2 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fl f(lambda)/f(5556 A) for component fl --- fk f(lambda)/f(5556 A) for component fk --- fc f(lambda)/f(5556 A) for component fc --- K3 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fl f(lambda)/f(5556 A) for component fl --- fd f(lambda)/f(5556 A) for component fd --- fc f(lambda)/f(5556 A) for component fc --- K5 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fl f(lambda)/f(5556 A) for component fl --- fd f(lambda)/f(5556 A) for component fd --- fk f(lambda)/f(5556 A) for component fk --- fc f(lambda)/f(5556 A) for component fc --- M0 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fk f(lambda)/f(5556 A) for component fk --- fm f(lambda)/f(5556 A) for component fm --- M1 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fd f(lambda)/f(5556 A) for component fd --- fk f(lambda)/f(5556 A) for component fk --- fm f(lambda)/f(5556 A) for component fm --- M2 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fl f(lambda)/f(5556 A) for component fl --- fk f(lambda)/f(5556 A) for component fk --- fsv f(lambda)/f(5556 A) for component fsv --- fm f(lambda)/f(5556 A) for component fm --- M3 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fl f(lambda)/f(5556 A) for component fl --- fd f(lambda)/f(5556 A) for component fd --- fm f(lambda)/f(5556 A) for component fm --- fsv f(lambda)/f(5556 A) for component fsv --- M4 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fl f(lambda)/f(5556 A) for component fl --- fm f(lambda)/f(5556 A) for component fm --- fsv f(lambda)/f(5556 A) for component fsv --- M5 III (1150-25000 A) M7 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fl f(lambda)/f(5556 A) for component fl --- fk f(lambda)/f(5556 A) for component fk --- fm f(lambda)/f(5556 A) for component fm --- M6 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fm f(lambda)/f(5556 A) for component fm --- M8 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fl f(lambda)/f(5556 A) for component fl --- fm f(lambda)/f(5556 A) for component fm --- M9 III (1150-25000 A) M10 III (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- K3-4 II (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fc f(lambda)/f(5556 A) for component fc --- M3 II (1150-25000 A) B8 I (1150-25000 A) F0 I (1150-25000 A) F5 I (1150-25000 A) K2 I (1150-25000 A) K3 I (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fl f(lambda)/f(5556 A) for component fl --- fse f(lambda)/f(5556 A) for component fse --- G0 I (1150-25000 A) lambda wavelength (in Angstroms) 0.1nm nflam component-averaged f(lambda)/f(5556 A) --- sdnflam std. dev. of avg. at this wavelength --- fh f(lambda)/f(5556 A) for component fh --- fse f(lambda)/f(5556 A) for component fse --- fk f(lambda)/f(5556 A) for component fk --- authorig.doc author's original distribution documentation srclist.doc summary of sources of published spectra complist.doc detailed info on sources forming each spectrum linecont.doc line and continuum definitions for LEW.TAB uifilt.doc filter transmission profiles U3,B2,B3,V,Rc,Ic jmfilt.doc filter transmission profiles J,H,K,L,L',M J. Weiland SSDOO/ADC 1998 Sept 03 Thanks to Dr. A. Pickles for comments and clarifications. UNKNOWN UNKNOWN Original files obtained from http://www.ifa.hawaii.edu/~pickles/hlib.html. Modifications included header text removal and some slight reformatting for column alignment in the *.dat files. J_PASP_110_863.xml 3CR Source Identifications, Update 1990 J/PASP/97/932 J/PASP/97/932 3CR Source Identifications 3CR Source Identifications, Update 1990 H Spinrad S Djorgovski J Marr L Aguilar Publ. Astron. Soc. Pac. 97 932 1985 1985PASP...97..932S Radio sources Redshifts This catalog contains the third major update of new optical and radio data for the strong sources in the Revised Third Cambridge Catalogue (3CR). Positions, redshifts, magnitudes, and identifications are included, as well as some radio data for 298 3CR sources.
catalog 3CR 3CR catalog number This columns gives the catalog number in the Revised 3CR Catalog of Radio Sources. --- RAh Right Ascension 1950 - hours h RAm Right Ascension - minutes min RAs Right Ascension - seconds s DE- Declination sign --- DEd Declination 1950 - degrees deg DEm Declination - arc minutes arcmin DEs Declination - arc seconds arcsec V V visual magnitude These columns contain information about the visual magnitude of the source. The mv column lists the visual magnitude of the object. If the mv is given in an even 0.5-magnitude interval, it has normally been estimated from the Palomar Sky Survey or direct photographic plates and therefore carries substantial errors (+/- 0.5-1.0 magnitude). An asterisk in the mvar_flg column indicates variability in mv with amplitude greater than 0.1 magnitude. mag Vflag [* ] variable magnitude flag --- z redshift --- S(178) flux density at 178 MHz from Kellerman et al Jy Alph spectral index These columns give information on the spectral index of the source. The spectral index given typically between 38 MHz and 750 MHz (see flags listed below) and is taken from Kellermann et al. (1969). The spectral index is defined as S prop. nu^(-alpha). --- b galactic lattitude --- r_ID reference for optical position The values refer to these references by number, and concern the origin of the optical identification, redshift, and radio map. --- r_z reference for redshift --- r_Radio reference for radio position --- notes Remarks on source This column gives additional information about the optical identification. For the optical identification we have generally listed the first published ID with a good finding chart. In cases where a previous paper without a good finding chart published the same ID or where the ID was confirmed by a subsequent, more detailed study, these references are listed under this column. In addition to listing additional information and redshift references, the remarks column gives other names (such as NGC number) and the character of the optical spectrum of radio galaxies using the following abbreviations: SE strong emission lines E emission lines present but not necessarily strong WE weak emission lines ABS only stellar absorption features are seen ABS remarks for QSOs indicates the presence of absorption features at one or more redshifts. Abbreviations used here include: CL cluster EF empty field FC finding chart G galaxy ID identification N NGC Q QSO SP spectrophotometry X indicates that the reference number preceding gives an incorrect * probable or possible identification or redshift --- ID IDentification of source These columns give information about the optical identification. The following abbreviations are used in the id column: B: BL Lac Object G: Galaxy N: N Galaxy Q: QSO --- list of references RefID Reference identification number --- RefText Reference text --- N.P.M. Kuin ADC/SSDOO/NASA 1995 Feb 14 UNKNOWN UNKNOWN The data were provided to the ADC on 1993-07-20 by Mark Dickinson for Hy i Spinrad. The documentation was updated with documentation written by D.E. Harris of SAO for the ADS version of this catalog. The ADS version includes extra fields: a Red Magnitude flag, a spectral index flag, and an identification flag. This catalog is also in the Andernach radio catalog archive as A035. J_PASP_97_932.xml Identifications and coordinates of variable stars in the globular cluster M 3 = NGC 5272. J/PAZh/20/693 J/PAZh/20/693 Identification and coordinates in NGC 5272 Identifications and coordinates of variable stars in the globular cluster M 3 = NGC 5272. N M Evstigneeva N N Samus T M Tsvetkova Yu A Shokin Pis'ma Astron. Zh. 20 693 1994 1994PAZh...20..693E V/97 : Updated 3rd Cat Variable Stars in Globular Clusters (Clement+ 1997) II/214 : Combined General Catalogue of Variable Stars (Kholopov+ 1998) Clusters, globular Positional data Equatorial coordinates of variable stars in the globular cluster NGC 5139=M3 and its nearest surroundings, mainly measured on a plate taken with The Zeiss-1000 telescope, are presented. Positions in a homogeneous system are presented for the first time for objects from the Catalogue of variable stars in globular clusters as well as for GCVS and NSV catalogue stars.
Coordinates of variables in M 3 (Tables 1-6 of the paper) Cat Published list source of stars number=1 1: Sawyer Hogg, 1973, Cat. <V/97>, Cl* NGC 5272 SAW VNNN in Simbad 2: Kholopov, P.N., 1963PZ.....14..275K, 1977PZ.....20..313K Cl* NGC 5272 X NN in Simbad 3: Sandage, 1953AJ.....58...61S, CL* NGC 5272 S AAAAA in Simbad 4: Kadla & Gerashchenko, 1980Tsir1123....1K, Cl* NGC 5272 KG NN in Simbad 5: von Zeipel, 1908AnPar..25....1V 6: Heinrich et al., 1967, Veroeff. Sternw. Tautenburg, 1, 1. --- Star Designation of the star in the list --- Zeipel von Zeipel (1908AnPar..25....1V) number --- NSV NSV (Cat. <II/214>) catalogue number --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Rem Remark on multiplicity See Note number=2 w,e,s,n,se,ne - components of pairs * - complex star system --- Veta Avedisova INASAN 1999 Feb 20 J_PAZh_20_693.xml New list of OB associations of our Galaxy. J/PAZh/21/13 J/PAZh/21/13 New list of OB associations New list of OB associations of our Galaxy. A M Melnik Yu N Efremov Pis'ma Astron. Zh. 21 13 1995 1995PAZh...21...13M Associations, stellar A new partition into associations of OB stars within 3kpc of the Sun is derived using Battinelli's modification of the cluster analysis method. We have found 58 associations, of which only 10% may be considered as a random clusters of field stars.
Table of OB-associations Name Association name --- GLON Galactic longitude deg GLAT Galactic latitude deg D Distance kpc RV Average radial velocity of the association relative to the Sun km/s e_RV Dispersion of RV km/s NRV Number of stars with measured RV --- Ntot Total number of stars in the association --- Dl Size of association along longitude pc Db Size of association along latitude pc p p=1, for the association with 90% reliability p=0 - reliability below 90% --- Nsg Number of K and M supergiants --- Veta Avedisova INASAN 1997 Jul 10 J_PAZh_21_13.xml Identifications and coordinates of variable stars in the globular cluster M 5 = NGC 5904. J/PAZh/21/509 J/PAZh/21/509 Identification and coordinates in M5 Identifications and coordinates of variable stars in the globular cluster M 5 = NGC 5904. N M Evstigneeva Yu A Shokin N N Samus T M Tsvetkova Pis'ma Astron. Zh. 21 509 1995 1995PAZh...21..509E Clusters, globular Positional data Accurate equatorial coordinates have been determined for 143 variable and suspected variable stars in the globular cluster M5=NGC 5904. For 28 stars, identifications with Kustner (1933VeUSB..26....1K) catalogue were found for the first time.
Coordinates of variables in M 5 Cat Published list source of stars number=1 1: Sawyer Hogg, 1973, Cat. <V/97>, Cl* NGC 5904 SAW VNNN in Simbad 2: Gerashchenko, 1987IBVS.3044....1G, Cl* NGC 5904 Saw VNNN in Simbad 3: Kravtsov, 1991PAZh...17.1101K, Cl* NGC 5904 Saw VNNN in Simbad 4: Arp, 1955AJ.....60..317A, Cl* NGC 5904 Arp R-NNN in Simbad 5: Buonanno et al., 1981MNRAS.196..435B, Cl* NGC 5904 ARP R-NNN in Simbad 6: Zhukov, L.V. 1971, TrPul 78, 160. --- Star Designation of the star in the list --- Kust Kustner (1933VeUSB..26....1K) number --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) number=2 Misprint in the paper has been corrected for Ref. 1, variable 48. s DE- Declination sign (J200.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Rem nw,se,e,w -components of pairs --- Veta Avedisova INASAN 1999 Feb 20 J_PAZh_21_509.xml Photographic photometry of stars and positions of variables in the globular cluster NGC 6584. J/PAZh/21/596 J/PAZh/21/596 BVR photometry of NGC 6584 Photographic photometry of stars and positions of variables in the globular cluster NGC 6584. N N Samus' A P Ipatov O M Smirnov V V Kravtsov G Alcaino W Liller F Alvarado Pis'ma Astron. Zh. 21 596 1995 1995PAZh...21..596S Clusters, globular Photometry, CCD Stars, variable Automatic stellar photographic BVR photometry reaching 1mag below the horizontal branch of NGC 6584, located at V~16.5mag, has been performed for this poorly studied globular cluster. One of the photoelectric standard stars used in our reductions appears to be variable. We also determined accurate coordinates of 52 variable stars in the cluster and around it.
NGC 6584 18 18 37.5 -52 12 55
Photographic photometry of stars in NGC 6584 Seq Sequential number --- Xpos X position arcmin Ypos Y position arcmin Vmag V magnitude mag B-V B-V colour index mag V-R V-R colour index mag Coordinates of variable stars Name Star identification according to Millis & Liller (1980AJ.....85..235M) or GCVS name (Cat. <II/139>) --- RAh Right ascension (2000.0) h RAm Right ascension (2000.0) min RAs Right ascension (2000.0) s De- Declination sign --- DEd Declination (2000.0) deg DEm Declination (2000.0) arcmin DEs Declination (2000.0) arcsec Xpos X position pix Ypos Y position pix James Marcout, Patricia Bauer CDS 1997 Jun 16 UNKNOWN UNKNOWN Prepared via OCR at CDS. J_PAZh_21_596.xml Rapid optical variability in NGC 7469: UBV photometry. J/PAZh/21/652 J/PAZh/21/652 Optical variability in NGC 7469 Rapid optical variability in NGC 7469: UBV photometry. V M Lyuty V T Doroshenko V G Metlov T R Irsmambetova Pis'ma Astron. Zh. 21 652 1995 1995PAZh...21..652L Galaxies, Seyfert Photometry, UBV The results of three-color UBV observations of rapid variability in the nucleus of the Seyfert galaxy NGC 7469 carried out in 1990-1994 are presented. The observations have been carried out during 15 different nights using the 60- and 125-cm telescopes with time resolution of 6-8min (50 hours monitoring) with the aperture of 27.5". The mean errors of one measurement are 1.8, 1.2 and 1.4% for U, B and V. The data set length during one night is from 2 up to 5h. The different nights show the variations at different level: from weak, when the standard deviation during the night exceeds the error of one measurement only by 10-20%, up to strong ones, when the standard deviation exceeds the error of the measurement by factor two.
NGC 7469 23 03 15.6 +08 52 29
UBV photometry of NGC 7469 HJD Julian date d Umag U magnitude mag Bmag B magnitude mag Vmag V magnitude mag Veta Avedisova INASAN 1999 Feb 01 J_PAZh_21_652.xml The giant branch and variable stars in the globular cluster NGC 3201. J/PAZh/22/269 J/PAZh/22/269 Giant branch and variable stars in NGC 3201 The giant branch and variable stars in the globular cluster NGC 3201. N N Samus V V Kravtsov M V Pavlov V V Strel'nikov Yu A Shokin G Alcaino W Liller F Alvarado Pis'ma Astron. Zh. 22 269 1996 1996PAZh...22..269S V/97 : Updated 3rd Cat Variable Stars in Globular Clusters (Clement+ 1997) Clusters, globular Photometry, photographic Stars, variable Accurate equatorial coordinates have been determined for variable stars in the globular cluster NGC 3201. Results of photographic BV photometry are presented.
Photographic photometry of stars in NGC 3201 Xpos X coordinate number=1 coordinates in the scale of the 1-m Swope telescope plates, x increases to the west, arbitrary origin, y increases to the south, arbitrary origin. mm Ypos Y coordinate number=1 coordinates in the scale of the 1-m Swope telescope plates, x increases to the west, arbitrary origin, y increases to the south, arbitrary origin. mm Vmag V magnitude mag B-V B-V color mag Coordinates of variables in NGC 3201 (Tables 3 and 4 of the paper) SAW Variable star number number=1 Variable star number is taken from the numbering system of Sawyer Hogg, H. 1973, Cat. <V/97>, Cl* NGC 3201 SAW VNN in Simbad --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Xpos x rectangular coordinate number=2 x, y rectangular coordinates are presented to facilitate identifications. mm Ypos y rectangular coordinate number=2 x, y rectangular coordinates are presented to facilitate identifications. mm Rem Remarks number=3 c - photometric center of a double; s, sw, ne - components of pairs. --- Veta Avedisova INASAN 1999 Mar 10 J_PAZh_22_269.xml Identification and coordinates of variable stars in the globular cluster M 4 = NGC 6121. J/PAZh/22/847 J/PAZh/22/847 Identification and coordinates in M4 Identification and coordinates of variable stars in the globular cluster M 4 = NGC 6121. Y A Shokin N N Samus Pis'ma Astron. Zh. 22 847 1996 1996PAZh...22..847S V/97 : Updated 3rd Cat Variable Stars in Globular Clusters (Clement+ 1997) Clusters, globular Positional data Stars, variable Accurate equatorial coordinates have been determined for 54 variable stars in the globular cluster M 4=NGC 6121.
Coordinates of variables in M 4 (Tables 1 & 2 of the paper) Star Star designation number=1 VNNNN: Number from Sawyer Hogg, H., 1973, Cat. <V/97>; Cl* NGC 6121 SAW VNN in Simbad ANNNN: Number from Alcaino, G., 1975A&AS...21....5A; Cl* NGC 6121 Alc NNN in Simbad LNNNN: Number from Lee, S.-W., 1977A&AS...27..367L --- Green Star number from Greenstein (1939) number=2 Stars from Greenstein' list (1939ApJ....90..387G) --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Rem SW, NE -components of a pair --- Veta Avedisova INASAN 1999 Mar 10 J_PAZh_22_847.xml On the origin of optical variability of WW Vulpeculae. J/PAZh/23/277 J/PAZh/23/277 Optical variability of WW Vul On the origin of optical variability of WW Vulpeculae. G V Zaitseva V M Lyutyi Pis'ma Astron. Zh. 23 277 1997 1997PAZh...23..277Z Photometry, UBV Stars, variable The UBV observations of WW Vul performed between 1983 and 1993 are presented. All UBV observations of WW Vul are reduced to GAISh photometric system.
WW Vul 19 35 59.6 +21 12 33
UBV photometry of WW Vul HJD Julian date d Vmag V magnitude mag B-V B-V color index mag U-B U-B color index mag Veta Avedisova INASAN 1999 Feb 15 J_PAZh_23_277.xml Analysis of flare activity in SS 433 on the basis of photoelectric photometry. J/PAZh/23/341 J/PAZh/23/341 BVR observations of SS 433 Analysis of flare activity in SS 433 on the basis of photoelectric photometry. T R Irsmambetova Pis'ma Astron. Zh. 23 341 1997 1997PAZh...23..341I Binaries, X-ray Photometry, UBVRI Photoelectric BVR photometry of SS 433 performed between 1988 and 1990 at Mt. Maidanak is presented.
SS 433 19 11 49 +04 58 34
BVR photometry of SS 433 JDH Julian date d Bmag B magnitude mag Vmag V magnitude mag Rmag R magnitude mag Veta Avedisova INASAN 1999 Feb 12 J_PAZh_23_341.xml Identification and coordinates of variable stars in the globular clusters M 53 = NGC 5024 and NGC 2808. J/PAZh/23/454 J/PAZh/23/454 Identification and coordinates in M 53 Identification and coordinates of variable stars in the globular clusters M 53 = NGC 5024 and NGC 2808. N M Evstigneeva N N Samus G Alcaino Pis'ma Astron. Zh. 23 454 1997 1997PAZh...23..454E V/97 : Updated 3rd Cat Variable Stars in Globular Clusters (Clement+ 1997) Clusters, globular Positional data Stars, variable Equatorial coordinates have been determined for 61 variables in the northern globular cluster M 53 and for 12 variables in the southern globular cluster NGC 2808 with accuracy sufficient for reliable identifications. A number of errors have been revealed in publications on variable starts in M 53.
Coordinates of variables in M53 and NGC 2808 (Tables 1 & 2 of the paper) NGC NGC number of the globular cluster --- Seq Sequential number of the star number=1 For NGC 5024, VNN: Sawyer Hogg, 1973, Cat. <V/97>, Cl* NGC 5024 SAW VNNN in Simbad KNN: Kravtsov, 1990ATsir1544...21K, Cl* NGC 5024 KRA NN in Simbad For NGC 2808, VNN: Clement & Hazen, 1989AJ.....97..414C, Cl* NGC 2808 Saw VNN in Simbad --- RAh Right ascension (J2000.0) h RAm Right ascension (J2000.0) min RAs Right ascension (J2000.0) s DE- Declination sign (J2000.0) --- DEd Declination (J2000.0) deg DEm Declination (J2000.0) arcmin DEs Declination (J2000.0) arcsec Comp ? Pair of components --- Veta Avedisova INASAN 1999 Mar 10 J_PAZh_23_454.xml The nature of visual components in 82 multiple systems J/PAZh/24/307 J/PAZh/24/307 Visual components in 82 multiple systems The nature of visual components in 82 multiple systems N I Shatsky Pis'ma Astron. Zh. 24 307 1998 1998PAZh...24..307S Photometry Stars, double and multiple The results of a BVR photometry observations are presented for multiple stars visual subsystems (table2.dat). The objects (table1.dat) were observed in 1996 with the 60 cm and 1 m telescopes at Maidanak Observatory (Uzbekistan) by aperture and scanning photometers. The positional parameters and physical relation of visual subsystems are also given (table4.dat).
Objects RAh Right Ascention, hours (2000) h RAm Right Ascention, minutes (2000) min RAs Right Ascention, seconds (2000) s DE- Declination sign --- DEd Declination, degrees (2000) deg DEm Declination, minutes (2000) arcmin DEs Declination, seconds (2000) arcsec IDS IDS-style designation --- ADS ADS number --- HD HD (Cat. <III/135>) number --- HR HR (Cat. <V/50>) number --- Components BVR photometry IDS IDS-style designation --- m_IDS Component(s) name --- Vmag 0.55 um mag e_Vmag Vmag error mag B-V B-V Color mag e_B-V B-V error mag V-R V-R Color mag e_V-R V-R error mag Nobs Number of observations --- Device Technique used number=1 a : aperture photometer s : scanning photometer --- Method Extinction Correction Method number=2 S : Object primary comp.-photometry used C : Correction by close standard D : Correction by distant standard M : Mean extinction correction V : Flux variation detected --- Subsystem parameters and status IDS IDS-style designation --- Sys Visual subsystem designation --- dVmag 0.55 um difference mag PA Positional angle deg Rho Separation arcsec Source PA-rho reference number=1 GSC : Guide Star Catalogue Hip : HIPPARCOS (Cat. <I/239>) Catalogue Tyc : TYCHO (Cat. <I/239>) Catalogue WDS : Washington Catalogue of Visual Double Stars (Cat. <I/237>) 4M : Carte du Ciel star - : approximate parameters are given --- Status Components relation number=2 P : physical system A : associated pair O : optical system criteria: h : by hypothetical parallax v : close pair: rho<3" p : by photometric parallaxes m : by proper motions r : by radial velocities ? : uncertainty flag --- Note *: remark in notes4.dat file --- Individual notes to table4.dat IDS IDS-style designation --- Com Comments --- Veta Avedisova INASAN 1998 Apr 06 J_PAZh_24_307.xml A reference catalog for accurate position determinations in the region of M 31 J/PAZh/24/93 J/PAZh/24/93 M 31 reference catalog A reference catalog for accurate position determinations in the region of M 31 Yu A Shokin N B Kulagina Pis'ma Astron. Zh. 24 93 1998 1998PAZh...24...93S http://nostromo.sai.msu.su/m31/ : The star chart Fundamental catalog Magnitudes Positional data We compiled a catalog of 421 references 12-15mag stars for determining accurate positions of objects in the region of M 31. We also compiled a star chart, which is provided as an Internet Web service, for identifying the catalogued reference stars on the plates of observers. AQccurate positions and a finding chart are given for 33 reference 15-17mag stars in a 10'x12' field near the center of M 31.
Reference catalogue [SK98] Sequential number --- Bmag Photographic B magnitude number=1 The photoelectric magnitudes for stars Nos. 195, 298, 225, 254 are from Arp, 1956AJ.....61...15A and for star 239 from de Vaucouleurs & Corwin, 1985ApJ...295..287D mag RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec Equatorial coordinates (B1950) of stars at the center of M31 [SK98]Center Number of reference star --- RAh Right ascension (1950) h RAm Right ascension (1950) min RAs Right ascension (1950) s DE- Declination sign --- DEd Declination (1950) deg DEm Declination (1950) arcmin DEs Declination (1950) arcsec GlC Globular cluster name number=1 Five objects in this table are globular clusters with numbers by Sargent et al., 1977AJ.....82..947S --- James Marcout, Patricia Bauer CDS Veta Avedisova INASAN 1998 May 19 UNKNOWN UNKNOWN //nostromo.sai.msu.su/m31/ J_PAZh_24_93.xml Identification of radio sources in clusters of galaxies. I. J/PAZh/25/447 J/PAZh/25/447 Identification of radio sources. I. Identification of radio sources in clusters of galaxies. I. A G Gubanov V P Reshetnikov Pis'ma Astron. Zh. 25 447 1999 1999PAZh...25..447G VIII/51 : The FIRST Survey, version 1998Feb (White+ 1998) Radio sources Clusters, galaxy Detailed identification of radio sources within the Abell radii in 26 rich galactic clusters of the FIRST catalog with optical objects of the APM and DSS surveys had been carried out. Of the 326 radio sources in the cluster fields, 99 are identified, 40 have probable identifications, and 187 are unidentified. Among last sources, 20 are definitely located in the clusters and 34 are cluster members with high probability. Thus, 30-40% of the FIRST radio sources could be identified using APM and DSS data, and there were two sources in each cluster on the average.
Summary of the radio sources [GR99b] Radio source name ([GR99b] ANNNN.NN in Simbad) --- note mark for probable sidelobes --- ro Distance from cluster center in units of Abell radius, (ro=r/Ra), --- RAh Radio right ascension (J2000) h RAm Radio right ascension (J2000) min RAs Radio right ascension (J2000) s DE- Radio declination sign (J2000) --- DEd Radio declination (J2000) deg DEm Radio declination (J2000) arcmin DEs Radio declination (J2000) arcsec Survey Radio survey name number=1 fst: FIRST survey nvs: NVSS survey --- Comp Radio component number --- Sfst 1400 MHz FIRST flux density mJy Snvs 1400 MHz NVSS flux density mJy RAoh Optical right ascension (J2000) h RAom Optical right ascension (J2000) min RAos Optical right ascension (J2000) s DEo- Optical declination sign (J2000) --- DEod Optical declination (J2000) deg DEom Optical declination (J2000) arcmin DEos Optical declination (J2000) arcsec a/d Optical survey name number=2 dss: DSS survey apm: APM survey --- C Optical filter number=3 R: for E-plate B: for Palomar O-plate --- mag Apparent magnitude mag Id Identification reliability number=4 Id: identified pld: probably identified NI: unidentified --- Cl Cluster membership number=5 C: in cluster pC: probably in cluster nC: not in cluster --- Veta Avedisova INASAN 1999 Mar 10 J_PAZh_25_447.xml